text:
\section{Introduction}

One of the main puzzles of Galactic microlensing surveys is the poorly
determined location of the lens population of the events towards the
Magellanic Clouds.  Currently there are two popular views on the
issue: (a) the lenses are located in the halo, hence are likely
baryonic dark matter candidates (Alcock et al. 1997); (b) both the
lenses and sources are part of the Magellanic Clouds, hence are stars
orbiting in the potential well of the Clouds (Sahu 1994, Wu 1994, Zhao
1998a,b, 1999a, Weinberg 1999).  These lead to drasticly different
predictions the relative amount of baryonic dark matter in galaxy
halos as compared to baryons in stars and gas of various phases in
galaxies and intergalactic medium.  Gould (1995) showed that the low
dispersion of many LMC tracers limits the amount of self-lensing in a
virialized disk of the LMC, as assumed in original models of Sahu and
Wu.  Zhao (1998a) suggested that this constraint can be circumvented
by invoking a plausible amount of unviralized material, particularly
tidally excited material in the immediate surrounding of the LMC disk,
as either foreground lenses or background sources.  Zhao (1998b)
suggested that the polar stream seen in Kunkel et al.'s (1997)
kinematic survey of the LMC carbon stars could contribute to lensing.
Weinberg (1999) showed a specific model for thickening the LMC disk by
interaction with the Galaxy.  Presently the observational status is
still very confusing.  Several observations suggest that our line of
sight to the LMC passes through a 3-dimensional stellar distribution
more extended in the line of sight than a simple thin disc of the LMC
(Kunkel et al. 1997, Zaritsky et al. 1997, 1999 and references
therein).  Zaritsky et al. (1999) also include a review of the
arguments and counter-arguments for these structures.

To break the degeneracy of the models we need new observations which
are sensitive to the thickness of the LMC and the location of the
lenses.  Several ways have been proposed, including studying the
spatial distribution and magnitude distribution of the microlensed
sources (Zhao 1999a, Zhao, Graff \& Guhathakurta 1999), the radial
velocity distribution of the sources (Zhao 1999b) and the reddening
distribution of the sources (Zhao 1999c).  Essentially if lensing is
due to Galactic halo machos or a foreground object, the sample of
lensed stars should be a random subsample of the observed stars in the
LMC.  On the other hand, if there are some tidal material behind the
LMC disk, then the stars in the tidal debris can be strongly lensed by
ordinary stars in the intervening LMC disk, hence the spatial and
kinematical distributions of these source stars will be those of the
tidal debris, rather than those of the LMC disk.  It is suggested that
the source stars in the tidal debris should stand out as outliers in
the radial velocity distribution of the LMC (Zhao 1999b), or
fainter-than-normal red clump stars in the color magnitude diagram
(Zhao, Graff \& Guhathakurta 1999).

The idea about the reddening distribution is to measure the distribution of the
reddening of individual LMC stars in small patchs of sky centered on
the microlensed stars.  Basicly some kind of ``reddening parallaxes''
can be derived for these stars from the line of sight depth effect,
i.e., the dust layer in the LMC makes stars behind the layer
systematicly redder than those in front of the layer.  The method
involves obtaining multi-band photometry and/or spectroscopy of fairly
faint ($19-21$mag) stars during or well after microlensing.
From these data we can infer the reddening of microlensed stars and
neighbouring unlensed stars.  The method, in some sense, is a variation
of the distance effect suggested by Stanek (1995) for the Galactic bulge
microlensing events.

Here we extend the analysis of Zhao (1999c) and present simulations of
the reddening of microlensed sources and show how reddening might be
used to constrain the macho fraction in the halo.  The models are
described in \S2, results are shown in \S3.  We summarize in \S4 and
discuss a few practical issues.

\section{Models}

\subsection{Density models for the dust, the stars and the lenses}

For the time being we shall assume a smoothed dust layer of the LMC
with a ${\rm sech}^{2}$ profile and a FWHM of $w$.
Let $\rho_{\rm d}(D)$ be the dust density at distance $D$, then
\begin{equation}\label{dustden}
\rho_{\rm d}(D) dD= \rho_{\rm d}(D_{\rm LMC}) {\rm sech}^{2} \left({D-D_{\rm LMC} \over 0.56 w}\right) dD,
\end{equation}
where $\rho_{\rm d}(D_{\rm LMC})$ is
the dust density at the mid-plane of the LMC.

For the LMC stars, we assume a two-component model.
Let $\rho_{\rm LMC}(D)$ be the density of the LMC stars, then
\begin{equation}
\rho_{\rm LMC}(D) = {\Sigma_{\rm disk} \over 0.56 W}
{\rm sech}^{2} \left({|D-D_{\rm LMC}| \over 0.56 W}\right) +
{\Sigma_{\rm extra} \over 1.06 W_{\rm extra}}
\exp\left[{-0.69 L^2}\right],
\end{equation}
where
\begin{eqnarray}
L &=& {(D_{\rm max}-D_{\rm min}) (D-D_{\rm extra})\over  (D_{\rm max}-D_{\rm extra})W_{\rm extra}},
~~{\rm if~} D_{\rm max}> D > D_{\rm extra},\\
  &=& {(D_{\rm max}-D_{\rm min}) (D-D_{\rm extra})\over  (D_{\rm extra}-D_{\rm min})W_{\rm extra}},
~~{\rm if~} D_{\rm min}< D < D_{\rm extra}.
\end{eqnarray}
Our LMC model includes a (thin) ${\rm sech}^{2}$-disk component of a surface
density $\Sigma_{\rm disk}$ and FWHM thickness $W$,
and an extra component with a surface density $
\Sigma_{\rm extra}$ and FWHM thickness $W_{\rm extra}$.  The extra
component consists of two half-Gaussians, which are joined together at their
peaks at $D=D_{\rm extra}$ and truncated at the lower and upper ends at
$D=D_{\rm min}$ and $D=D_{\rm max}$.  This is intended to model any
non-virialized material in the vicinity of the LMC (Zhao 1998a, Weinberg 1999).
To be most general, an offset between the extra component and
the LMC disk, namely $D_{\rm extra} \ne D_{\rm LMC}$, is allowed in our models.

Let $\nu_*(D)dD$
be the number of LMC star in a line of sight distance bin ($D$, $D+dD$),
then the LMC star number density will be given by
\begin{equation}\label{nustar}
\nu_*(D)dD = C_0 \rho_{\rm LMC}(D) D^2 dD,
\end{equation}
where $C_0$ is a normalization constant.

For the lens population, we include the contribution from the LMC stars
and  intervening machos in an isothermal
halo.  The density of lenses at distance $D_l$ is
\begin{equation}\label{lensden}
\rho_{\rm lens} (D_l) =
\rho_{\rm LMC}(D_l) + f_{\rm macho} \rho_{\rm halo}(D_l),
\end{equation}
where
$f_{\rm macho}$ is the fraction of machos in the halo, and
$\rho_{\rm halo}(D)$ is the dark halo density given by
\begin{equation}\label{halo}
\rho_{\rm halo}(D) = 0.01M_\odot {\rm pc}^{-3}
\left[ 1+\left({D \over 8{\rm kpc}}\right)^2 \right]^{-1}.
\end{equation}
The halo density corresponds to
a surface density of dark matter (machos plus wimps) halo
$\Sigma_{\rm halo} \sim 100M_\odot\,{\rm pc}^{-2}$ towards the LMC.

\subsection{Reddening vs. line of sight distance of a star
and their distributions}

In general the reddening of a star is correlated with the distance to
the star, with stars at the backside of the LMC seeing more dust and
experiencing more reddening.  But since the dust distribution is
clumpy and the reddening distribution is patchy, any relation between
the reddening and the line of sight distance is not a well-defined
one-to-one relation, but has a significant amount of scatter due to
patchiness of dust and measurement error.  Nevertheless we can argue
that stars in a small (e.g., $4'' \times 4''$) patch of sky will see
the same set of dust clouds, so if we sort these neighbouring stars
according their reddening, we also get a sorted list in distance.

Stars in the LMC can be ranked according to an observable reddening indicator
$\kappa_{\rm obs}$.  For any LMC star define
\begin{equation}\label{kobs}
\kappa_{\rm obs} \equiv
{E(B-V)_{\rm LMC}^{\rm obs} \over \left<E(B-V)_{\rm LMC}^{\rm obs}\right>},
\end{equation}
where
$E(B-V)_{\rm LMC}^{\rm obs}$ is the observed reddening in $B-V$ color towards
the LMC star, after discounting the reddening by the Galactic foreground, and
$\left<E(B-V)_{\rm LMC}^{\rm obs}\right>$ is the average over random stars
in the small patch of sky centered on that LMC star,
and is approximately the reddening of those stars at the mid-plane of the LMC.
Surely the typical reddening
$\left<E(B-V)_{\rm LMC}^{\rm obs}\right>$ varies widely from patches
to patches on scales of arcmins (Harris et al. 1997 and references therein),
but the rescaled reddening
$\kappa_{\rm obs}$ allows us to sort the stars
not only in the same patch but also stars in different patches.
A higher rank, i.e. a larger $\kappa_{\rm obs}$,
means a deeper penetration into the dust layer.
Stars at the midplane have a rank
$\kappa_{\rm obs}=1$, and those at the front or back side of the LMC disk
have a rank $\kappa_{\rm obs}=0$ or $\kappa_{\rm obs}=2$.

Consider the reddening rank of stars in a smooth dust model.
Let $A_{\rm LMC}(D)$ be the dust absorption towards a LMC star at distance $D$
(after discounting the absorption by the Galactic foreground dust),
and let $\kappa(D)$ be the predicted reddening rank of the star, then
\begin{equation}
\kappa(D) = {A_{\rm LMC}(D) \over A_{\rm LMC}(D_{\rm LMC})}=
{\int_0^{D} \!\! \rho_{\rm d}(D) dD \over
\int_0^{D_{\rm LMC}} \!\! \rho_{\rm d}(D) dD}
\end{equation}
(cf eq.~\ref{dustden}),
where $\rho_{\rm d}(D_{\rm LMC})$ and $A_{\rm LMC}(D_{\rm LMC})$ are
the dust density and absorption at the mid-plane of the LMC.
It is easy to show that
\begin{eqnarray}\label{kd}
\kappa(D) &=& 1+\tanh \left({D-D_{\rm LMC} \over 0.56 w}\right)\\
	  &=& 0,~~~D-D_{\rm LMC} \ll w\\
          &=& 1,~~~D=D_{\rm LMC} \\
	  &=& 2,~~~D-D_{\rm LMC} \gg w.
\end{eqnarray}
So the reddening rank $\kappa(D)$ increases from 0 to 2 abruptly
in the distance range $D_{\rm LMC} \pm {w \over 2}$ as a star enters and exits
the dust layer.  It turns out that this property is not limited to
${\rm sech}^{2}$ profile dust, but generic for smooth dust layer of a symmetric
profile.

Now to take into account of the scatter due to measurement error and
any residual patchiness, we assume that the observed reddening has
a simple Gaussian distribution centered on the predicted value from a smooth
dust disk model.  Then for a star at any distance $D$, the reddening rank
$\kappa_{\rm obs}$ is drawn from the following distribution function
\begin{equation}\label{broad}
B(\kappa_{\rm obs}, D) = {1 \over \sqrt{2\pi} \sigma}
\exp \left[-{ \left(\kappa_{\rm obs}-\kappa(D)\right)^2 \over 2 \sigma^2}\right],
\end{equation}
which is a Gaussian with a constant dispersion $\sigma$, and a mean
$\kappa(D)$ as predicted from a smooth model.

Now we integrate over LMC stars at all distance and
bin them according to their reddening $\kappa_{\rm obs}$.
Let $N_*(\kappa_{\rm obs})$
be the relative frequencies of finding an unlensed star
with a reddening $\kappa_{\rm obs}$, then
\begin{equation}\label{ns}
N_*(\kappa_{\rm obs}) =  \int dD \nu_*(D)
B(\kappa_{\rm obs}, D).
\end{equation}

\subsection{Optical depth as a function of distance and reddening}

The microlensing optical depth
$\tau(D_s)$ of a source star at distance $D_s$ is defined by
\begin{equation}
\tau(D_s) \equiv {\nu_s(D_s) \over  \nu_*(D_s) }
\end{equation}
where $\nu_*(D_s)dD_s$ and
$\nu_s(D_s)dD_s$ are the numbers of stars and microlensed sources
in the distance bin ($D_s$, $D_s+dD_s$) respectively (cf. eq.~\ref{nustar}).
It is well-known that in the standard
full-macho isothermal halo model $f_{\rm macho}=1$,
$\rho_{\rm lens}=\rho_{\rm halo}$ (cf. eq.~\ref{lensden}), and
the microlensing optical depth $\tau_{\rm std}=5\times 10^{-7}$
(cf. e.g., Paczy\'nski 1986).  It is convenient to rescale the optical
depth of a model with this standard value.  The microlensing optical depth
$\tau(D_s)$ is then given by
\begin{equation}
\tau(D_s) =\tau_{\rm std} {
\int_{0}^{D_s} \!\! dD_l \rho_{\rm lens}(D_l) {(D_s -D_l)D_l/D_s}
\over
\int_{0}^{D_{\rm LMC}} \!\! dD_l
\rho_{\rm halo}(D_l) {(D_{\rm LMC} -D_l)D_l/D_{\rm LMC}}
}.
\end{equation}

The optical depth $\tau(D_s)$ increases with the source distance.
Suppose all lenses are at distance
$D_l$, then
\begin{equation}\label{tauprop}
\tau(D_s) \sim (D_s - D_l).
\end{equation}

Unfortunately, it is difficult to observe this effect because it is
hard to measure the distance to a LMC star at the accuracy of 1 kpc.
But fortunately the distance to a star is correlated with the
reddening, and the reddening of a star can be measured accurately to
20\%.  So we have an interesting effect that the rate of microlensing
is correlated with the reddening of the stars.  For each bin in terms
of the rank of reddening ($\kappa_{\rm obs}$, $\kappa_{\rm
obs}+d\kappa_{\rm obs}$), we can define an optical depth
\begin{equation}
\tau_{\rm obs}(\kappa_{\rm obs})
\equiv {N_s(\kappa_{\rm obs}) \over N_*(\kappa_{\rm obs})}
={\int dD_s \nu_s(D_s) B(\kappa_{\rm obs}, D_s)
 \over \int dD \nu_*(D) B(\kappa_{\rm obs}, D)},
\end{equation}
where
$N_*(\kappa_{\rm obs})$ and $N_s(\kappa_{\rm obs})$
are the relative frequencies of finding an unlensed star and
a microlensed source with reddening $\kappa_{\rm obs}$ respectively
(cf. eq.~\ref{ns}).

Note $\tau_{\rm obs}(\kappa_{\rm obs})$ is a function
measurable observationally because we can always bin the microlensed events
according their observable reddening, and get their frequencies
$N_*(\kappa_{\rm obs})$ and $N_s(\kappa_{\rm obs})$.  Of particular interest is
$\tau_{\rm obs}(0<\kappa_{\rm obs}\le 1)$.
Note stars at the mid-plane of the LMC disk have
average reddening, so $\kappa_{\rm obs} \sim 1\pm 3\sigma$ at
$3\sigma$ confidence level.  In comparison stars well in
front of the dust layer have $\kappa_{\rm obs}<3\sigma$, and stars
well behind the dust layer have $\kappa_{\rm obs}>2-3\sigma$.  So
$\tau_{\rm obs}(0<\kappa_{\rm obs}\le 1)$ is the optical depth of
a thin layer of stars co-spatial with the dust layer and slightly closer to us
the mid-plane of the LMC with $D_{\rm LMC}-w/2 \le D \le D_{\rm LMC}$.
Since the thickness of the dust layer $w \sim 100-200$pc is very small,
these stars are virtually at the same distance.
So we have
\begin{equation}\label{tobs1}
\tau_{\rm obs}(0 <\kappa_{\rm obs}\le 1)
\approx \tau(D_{\rm LMC}) \ge
f_{\rm macho}\tau_{\rm std}.
\end{equation}
So we have turned the theoretical quantity $\tau(D_{\rm LMC})$ to
an observable, and this observable optical depth
$\tau_{\rm obs}(0<\kappa_{\rm obs}\le 1)$
sets an upper limit on the amount of machos in the foreground of the LMC.
The above inequality reduces an equality
in the absence of any LMC lenses in front of the LMC disk.

If the picture that the LMC is a thin disk without any extra material
in the front or back is correct, then we should find that $\tau_{\rm
obs}(\kappa_{\rm obs})$ is at a constant level
$\approx \tau(D_{\rm LMC})= f_{\rm macho}\tau_{\rm std}$
for all reddening.

Presently the survey teams have not studied the reddening dependence
of the optical depth, so they quote only the observed optical depth
averaged over all LMC stars, which is only one number.
Let this be $\left< \tau_{\rm obs} \right>$, then current data require
\begin{equation}\label{tobs}
\left< \tau_{\rm obs} \right> \equiv
{\int_{D_{\rm min}}^{D_{\rm max}}\!\! dD \nu_*(D) \tau(D)
\over \int_{D_{\rm min}}^{D_{\rm max}}\!\! dD \nu_*(D) }
={\int\!\! d\kappa_{\rm obs} N_*(\kappa_{\rm obs}) \tau(\kappa_{\rm obs})
\over \int\!\! d\kappa_{\rm obs} N_*(\kappa_{\rm obs}) }
\approx 0.5 \tau_{\rm std},
\end{equation}
where the factor $0.5$ comes from the fact
that the observed microlensing optical
depth account for about one-half of that of the standard macho dark halo model
$\tau_{\rm std}$ (Alcock et al. 1997).

We would like to know how much of the observed optical depth
is due to stellar lenses in the LMC vicinity and how much
is due to machos in Galactic halo.
If we define $f_*$ as the fraction of the observed
microlensing depth due to stellar lenses, then the fraction of
machos in the dark halo is given by
\begin{equation}\label{fstar}
f_{\rm macho} = {\left< \tau_{\rm obs} \right> (1-f_*)
\over \tau_{\rm std}} = 0.5 (1-f_*).
\end{equation}
So for a given set of stellar distribution parameters $\Sigma_{\rm
extra}$ etc, we can predict the optical depth due to stellar lenses
$f_*\tau_{\rm std}$, we can then determine
$f_{\rm macho}$ by fixing the overall optical depth to the
observed value.

Finally we would like to characterize
the excess reddening of the microlensed stars.
This can be done by defining an observable parameter
$\xi_{\rm obs}$ such that
\begin{eqnarray}
\xi_{\rm obs} &\equiv &
{\int \! \! d\kappa_{\rm obs} N_s(\kappa_{\rm obs}) \kappa_{\rm obs}\over
 \int \! \! d\kappa_{\rm obs} N_s(\kappa_{\rm obs}) }-
{\int \! \! d\kappa_{\rm obs} N_*(\kappa_{\rm obs}) \kappa_{\rm obs}\over
 \int \! \! d\kappa_{\rm obs} N_*(\kappa_{\rm obs}) }\\
&=&
{\int \! \! dD \nu_s(D) \kappa(D) \over
 \int \! \! dD \nu_s(D)  }-
{\int \! \! dD \nu_*(D) \kappa(D) \over
 \int \! \! dD \nu_*(D)  }.
\end{eqnarray}
Because of the integration over the entire range of the reddening,
$\xi_{\rm obs}$ is independent of the dispersion $\sigma$
between the observed reddening rank of a star and the reddening rank
predicted from a smooth model
(cf. eq.~\ref{broad}).

\section{Results}

\subsection{Model parameters}

Here we study the effect of a mixed halo model on the reddening
distribution of the microlensed stars.  Since the parameters of the
LMC are very uncertain, we will explore a range of dust models and
stellar models.  Table 1 lists the parameters for the models.

We fix the distance to the LMC $D_{\rm LMC}=50$kpc, and set the tidal
radius of the LMC $|D_{\rm min}-D_{\rm LMC}|=|D_{\rm max}-D_{\rm
LMC}|=10$kpc.  For the ${\rm sech}^{2}$ stellar disk of the LMC and the dust
layer, we fix $\Sigma_{\rm disk}=400M_\odot{\ \rm pc}^{-2}$.  We fix
the FWHM thickness of the dust layer $w=200$ pc, but allow the
relative thickness of the two disks $W/w$ to vary in the range 0.5 to
2, a reasonable range for thin stellar and dust disks.  We set the
FWHM of the tidal material $W_{\rm extra}=0.05(D_{\rm max}-D_{\rm
min})=1$kpc, but allow the peak position to vary in the range 40 kpc
$\le D_{\rm extra} \le$ 60 kpc, and the amount of stars in extra
component to vary in the range $0 \le \Sigma_{\rm extra} \le
50M_\odot\,{\rm pc}^{-2}$.  We set this upper limit for the surface
density of the extra material to about $10\%$ of the surface density
of the LMC, an acceptable amount for some hidden material.  In
comparison the surface density of dark matter (machos plus wimps) halo
$\Sigma_{\rm halo} \sim 100M_\odot\,{\rm pc}^{-2}$ (cf. eq.~\ref{halo}).
These parameters are comparable to those of previous models for the volume
density of the LMC disk (Wu 1995, Weinberg 1999).

It turns out the reddening distributions of microlensed and unlensed
stars are insensitive to exact values of $w$, $W$, $W_{\rm extra}$ and
$\Sigma_{\rm disk}$ as long as we are in the regime where $w \sim W
\ll W_{\rm extra} \ll |D_{\rm max}-D_{\rm min}|$ and $\Sigma_{\rm
extra} \sim \Sigma_{\rm halo} \ll \Sigma_{\rm disk}$.
These distributions are more sensitive
to the ratios such as $W/w$, $\Sigma_{\rm extra}/\Sigma_{\rm halo}$,
and $|D_{\rm extra}-D_{\rm LMC}| \over |D_{\rm max}-D_{\rm min}|$.
For example, models with the extra stars centered on the LMC disk,
i.e., ${|D_{\rm extra}-D_{\rm LMC}| \over |D_{\rm max}-D_{\rm min}|}
\sim 0$, require much more stars with $\Sigma_{\rm extra}/\Sigma_{\rm
halo} \gg 1$ for come up with enough events, hence are much less
efficient than models with extra stars $5-10$kpc in front or behind
the LMC in terms of producing microlensing.
So the main parameters that we will vary are
$\Sigma_{\rm extra}$, $D_{\rm extra}$ and $W/w$.
The predictions are made for halo-lensing models and mixed models with
different amount of stars in the extra component and different offset
distance from the LMC and the relative thickness of the stellar disk
vs. the dust disk.

We also set the random error $\sigma$ for the observed reddening
at 20\%-40\% level, which seems a reasonably amount.  A larger
dispersion would smooth out some tell-tale features of the reddening
distributions.  But it turns out that the mean excess $\xi_{\rm obs}$
and and the optical depth in the mid-plane $\tau_{\rm obs}(\kappa_{\rm
obs}=1)$ are insensitive to the observational error $\sigma$.

\subsection{Reddening distributions of microlensed and unlensed stars}

The line of sight distributions of a few model quantities are shown in
Fig.~\ref{den.ps} for one of the models (see caption).  Clearly all
stellar density distributions peak at $D=D_{\rm LMC}=50$kpc, the
mid-plane of the high density disk of the LMC; similarly for the thin
dust layer.  The LMC stars have a second peak due to extra stars
placed behind the LMC disk.  The lens density distribution also has a
gentle falling part in the range 10 kpc $<D<$ 40 kpc due to foreground
machos, whose number density falls as $D^{-2}$.  The lensed stars
(dotted line with diamonds) also have a higher tail.

For sources in front the LMC disk $D<D_{\rm LMC}$ the microlensing
optical depth is nearly constant, $\tau(D_s)/\tau_{\rm std} \sim f_{\rm macho}
\sim 0.36$.  This is because the optical depth due to
the ever decreasing density of the foreground machos is insensitive to
the source distance.  But after passing the LMC disk the optical depth
takes off linearly with the source distance till $\tau(D_s)/\tau_{\rm std}
\gg 1$.  This is because any source star behind the LMC suddenly sees
an intervening dense screen of lenses coming from the high surface
density stellar disk of the LMC, so the optical depth goes up
in proportional to the distance to the LMC disk (cf. eq.~\ref{tauprop}).
This explains
the higher tail of the lensed stars as compared to unlensed stars
(cf. Fig.~\ref{den.ps}).  Note that there is only a modest increase
of the optical depth from entering to exiting the LMC thin disk.
The amount is on the order of
$(\Sigma_{\rm disk}/\Sigma_{\rm halo})(W/10{\rm kpc})<8\%$ of the total
optical depth, consistent with
the estimation of Sahu (1994) and Wu (1994) for a thin disk.

The dust extinction is nearly a Heaviside function of the distance,
climbing steeply from zero absorption in front of the layer to a
constant value $2\times A_{\rm LMC}(D_{\rm LMC})$ a few hundred pc
behind the layer, where $A_{\rm LMC}(D_{\rm LMC})$ is the absorption
in the mid-plane.  This is because as a star sinks deeper in the dust
layer it experiences an increasing reddening before it emerges from the
dust layer again.

Fig.~\ref{redist.ps} shows the reddening distributions of microlensed
and unlensed stars.  The distribution for unlensed stars (upper
panels) hardly depends on parameters of the extra component
$\Sigma_{\rm extra}$ and $D_{\rm extra}$.  It is only sensitive to the
relative thickness of the stellar disk and the dust layer.  At one end
of the extreme, we have a thin dust layer and a thicker stellar disk
($W/w=2$, solid lines).  We see the familiar double-horn structure.
This is because most stars in a thick disk are either in front of the
dust layer and free from reddening or behind the layer and reddened by
the maximum amount.  At the opposite extreme, if the stellar disk is
thinner than the dust layer ($W/w=0.5$, dash-dot-dot-dot lines), the
distribution becomes peaky in the middle because most stars of the
thin disk are in the mid-plane of the dust layer, hence reddened by
half of the maximum (back-to-front) value.  In between if the dust
layer and the stellar disk have the same scale height and are evenly
mixed ($W/w=1$, dashed lines), we have a flat top-hat distribution.

The distributions for the microlensed stars depend on the location and
the amount of the extra component.  For halo-lensing models, the
distribution of lensed stars and unlensed stars are virtually
indistinguishable (cf. Fig.~\ref{redist.ps}a).  The situation is
largely unchanged if we move all lenses from the halo to 10 kpc in
front of the LMC disk (cf. Fig.~\ref{redist.ps}b).  The extra
component shows up merely as a marginal excess of low reddening stars in the
unlensed stars, a small effect which might escape detection.

The situation is drasticly different if we put even a small amount
($\Sigma_{\rm extra}=10M_\odot\,{\rm pc}^{-2}$, or 2.5\%) of stars behind the
LMC disk (Fig.~\ref{redist.ps}c).  The distribution are strongly
skewed towards high reddening.  This is because lensing favors source
stars well-behind the lenses.  More specificly if the lenses are
machos midway to the LMC, or stars some 10 kpc in front of the LMC,
then the probability of drawing a source star at 100 pc behind the
dust layer is about 0.8\% or 2\% higher than drawing one at 100 pc in
front of the dust layer (cf. eq.~\ref{tauprop}).  So in average, the
lensed sources should be more reddened than the unlensed ones by
merely a few percent.  In contrast, if the lenses are at mid-plane of
the LMC, then nearly all sources will be behind the dust layer, and
hence the reddening rank $\kappa_{\rm obs}$ increases by one
(cf. eq.~\ref{kobs} and eq.~\ref{kd}).

In Fig.~\ref{redist.ps}c there are still some source stars at low
reddening because we allow for machos in the foreground.  The skewness
effect becomes stronger as we decrease the macho fraction, and
increase the extra stars behind the LMC.  For $\Sigma_{\rm
extra}=40M_\odot\,{\rm pc}^{-2}$ and $D_{\rm extra}=60$kpc, then all
lensed sources should have an observed reddening rank $\kappa_{\rm
obs} \approx 2$.  In this case $f_{\rm macho} \approx 0$ and all
lenses come from the LMC disk.

Another way to quantify the above effects is to look at the observed
optical depth as a function of the reddening rank of stars
(cf. Fig.~\ref{opt.ps}a).  The plateau of the $\tau_{\rm
obs}(\kappa_{\rm obs})$ curves in the range $0<\kappa_{\rm obs}\le 1$
are for stars imbeded in the dust layer of the LMC.  They are slightly
closer to us than the stars at the mid-plane, for which $\kappa_{\rm
obs}=1\pm 3\sigma$, but are virtually at the same distances $D_{\rm
LMC} \pm w/2$.  The plateau also set an upper limit on the optical
depth of machos (cf. eq.~\ref{tobs1}).

On the other hand those stars with $\kappa_{\rm obs} \ge 2$ include
both stars well behind the LMC disk, which have a very high optical
depth (cf. the curve of $\tau(D)$ in Fig.~\ref{den.ps}), and any
Gaussian tail of the LMC disk stars due to random error of the
reddening.  So $\tau_{\rm obs}(\kappa_{\rm obs})$ can have a high tail
if the extra component behind the LMC is stronger than the Gaussian
tail due to a non-zero dispersion $\sigma$.  These results depend
somewhat on the reddening and the relative thickness of the stellar
disk and the dust layer (cf. Fig.~\ref{opt.ps}b).  A larger
measurement error smoothes the sharp transition from the plateau to
the high tail.  The tail is lower if the stellar disk is thicker than
the dust layer, because of more overlap in the observed reddening of
the stars in the LMC disk and those well-behind the LMC.

Fig.~\ref{fmacho.ps} shows that in general a strong excess in
reddening is seen in models with most of the lenses in the LMC disk,
and the sources behind the midplane of the LMC disk.  Models with a
high macho fraction $f_{\rm macho} \ge 0.4$ and/or with lenses being
extra stars a few kpc well in front of the LMC disk predict only a
modest amount of excess $\xi_{\rm obs} \le 0.1$.  So these models
could be ruled out if we measure a strong excess.  In particular, if
$\xi_{\rm obs} \ge 0.5$ then the dark halo cannot have more than 15\%
in machos.  On the other hand, if the excess is small, then the
interpretation remains non-unique.  These results depends only
slightly on the thickness of the dust layer with the thinner dust
layer predicting a stronger excess.  Given accurate reddening, it is
possible to measure or at least set an upper limit on the fraction of
dark matter in machos.

\subsection{Empirical relations}

We have also find a few empirical relations for converting the
reddening excess $\xi_{\rm obs}$ to the macho fraction $f_{\rm macho}$.
Assuming that there
are few stellar lenses in the immediate foreground of the LMC disk,
which would be the case if $0.8 \ge \xi_{\rm obs} \ge 0.2$, then to a good
approximation, the fraction $f_*$ of microlensing due to LMC stars is given by
\begin{equation}
f_* \approx 1.2\xi_{\rm obs}.
\end{equation}
The fraction of machos is related to $\xi_{\rm obs}$ by
\begin{equation}
f_{\rm macho} \approx 0.5(1-1.2\xi_{\rm obs})
\end{equation}
(cf. eq.~\ref{fstar} and ~\ref{tobs}).
Here we have adopted the present reported value
for the microlensing optical depth
to the LMC, i.e., about half of that of the standard halo.
But the results can be rescaled proportionally as more data become available.

The result can also be recast as following,
\begin{equation}
f_{\rm macho}
\approx {\tau_{\rm obs}(0<\kappa_{\rm obs}\le 1)
\over 5\times 10^{-7} }
\end{equation}
(cf. eq.~\ref{tobs1}), where
$\tau_{\rm obs}(0<\kappa_{\rm obs}\le 1)$ is the optical depth of
the LMC stars observed with lower than average reddening; these are
stars sandwiched in a thin layer
between the mid-plane of the LMC disk and the near side of the dust layer.
The optical depth of the least reddened stars best approximates
the optical depth of foreground machos, because it is least contaminated
by stellar lenses in the LMC.

These relations work best if we can neglect stellar lenses in the
immediate foreground of the LMC disk.  But interestingly, these results
are insensitive to the assumption of the dust distribution and stellar
distribution of the LMC, e.g., the distance of the extra background
material, and their surface density, the relative thickness of the
dust layer and the stellar disk.  We also allow for a realistic amount
of measurement error and patchiness of extinction.

\section{Summary}

In summary, we have studied effects of dust layer in the LMC on the
microlensing events in a wide range of models of star and dust
distributions in the LMC.  We propose to bin LMC stars according to
their reddening rank $\kappa_{\rm obs}$ (as defined in
eq.~\ref{kobs}), and study the observable microlensing optical depth
as a function of the reddening rank $\kappa_{\rm obs}$.  We find that
self-lensing models of the LMC draw preferentially sources behind the
dust layer of the LMC, and hence can be distinguished from the
macho-lensing models once the reddening by dust is measured.

If a low excess in reddening ($\xi_{\rm obs}<0.2$) is observed then the
interpretation would not be unique: the reddening distribution does
not distinguish very well lensing by machos and lensing by stars a few
kpc in front of the LMC.  The optical depth can be explained equally
well by a screen of macho lenses with $\Sigma_{\rm extra}=50M_\odot\,{\rm
pc}^{-2}$ at 10 kpc from the Sun, or by a screen of stellar lenses
with a same surface density at 10 kpc in front of the LMC disk.  As
far as the reddening distributions are concerned, these two models are
barely distinguishable (cf. Fig.~\ref{redist.ps}ab).  On the other
hand the reddening distribution is very sensitive to any stars behind
the LMC disk.  If 2-3\% of the LMC stars is put in an extra component $5-10$
kpc behind the LMC, then we can see markedly different distribution in
the microlensed stars (cf. Fig.~\ref{redist.ps}c); this corresponds to
a surface density $\Sigma_{\rm extra}=10M_\odot\,{\rm pc}^{-2}$.  The
signal gets even stronger as we decrease the macho fraction and
increase the surface density of the background stars.

Our main finding is that among stars of different reddening rank,
the optical depth of the least reddened stars
$\tau_{\rm obs}(\kappa_{\rm obs} \sim 0)$ is the closest approximation to
the optical depth of machos (cf. Fig.~\ref{opt.ps}).
The macho fraction $f_{\rm macho}$ also correlates
tightly with the excess reddening $\xi_{\rm obs}$ of the microlensed sources
(cf. Fig.~\ref{fmacho.ps}).
These results are summarized by the
empirical relations in the previous section.  An observable high
excess in reddening ($1> \xi_{\rm obs} >0.2$) would be a definative signal for
many LMC disk lenses and low macho fraction.  Potentially we can
constrain the fraction of Galactic dark matter in machos this way.

There are a number of problems to apply the method to observations.
(a) Reddening of individual stars is difficult to measure accurately.
Reddening can be determined by constructing reddening-free indices
with photometry of three or more broad bands, or with low resolution
spectroscopy. Typical accuracy is about $0.02$ mag. in $E(B-V)$
with these methods (Harris et al. 1997),
which is about 20\% of the typical reddening in the LMC (Harris et al. 1997).
(b) Stars in the LMC are likely crowded from the ground.
Blended images of stars lead to unphysical colors and spurious
reddening.  (c) Dust distribution is very clumpy.  Extinction towards
OB stars in the LMC disk can
easily vary at a factor of two level among different patches of the
sky separated by $1'$ (Harris et al. 1997).
(d) The effect of extinction by the dust layer of the
Galaxy near the Sun should be included.
Oestriecher et al. (1996) show that the Galactic foreground extinction
is not entirely smooth.  There are dark patches on $30'$ scales.

The clumpiness of the dust, together with the fairly large error of the
reddening vector measurable from broad-band photometry, can lead to a
large scatter in the relation between reddening and line of sight
depth.  Zhao (1999c) argue that these problems, particularly
patchiness can be overcome if we restrict to the smallest patches of
sky around each microlensing source where the variation is likely at
only 20\% level.  Spectroscopic observation with the Hubble Space
Telescope in the ultra-violet can in principle resolve many faint
stars in the small patches around each microlensed stars, and measure
the reddening accurately.  By obtaining the reddening of stars in the present
$20-30$ microlensing lines of sight we
should be able to measure the excess reddening confidently.
We should also be able to bin the events in the reddening rank, and study
the optical depth as a function of reddening.  A null result of any
variation of the optical depth would be in favor of
a significant baryonic dark component of the Galaxy.

\vskip 1cm

\vfill \eject

\input tab1.tex

\input tab2.tex

\vfill \eject

redpajama_set_name: RedPajamaArXiv


We had a mega busy weekend, with family staying with us for the extended bank holiday weekend to celebrate the Jubilee of Old Queenie. Us being not particularly royally inclined just had a bit of a rest and used it as an excuse to drink some nice sparkly wine with friends and family and that was all lovely.
I woke up this morning ready to go to work and the day started very well, with tops that had been cut out the night before getting stitched together and I was feeling all warm and happy at the lovely colour combinations and having some fun with the embroidery when Bertha decided to start to protest. She made some unhealthy noises and seemed to be a bit stiff in her metal joints and then she kept missing stitched and snarling up the thread. So she has gone off to get some TLC at the hospital for tired and overworked mechanical friends.


text:
Home Category Ducati
Latest News From Indian Automobile Industry – Ducati, BMW X7, Yamaha FZ 25, Mercedes-Maybach GLS600
by sudhir
Ducati Multistrada 950 S GP White Launched In India: Priced At Rs 15.69 Lakh
Latest News From Indian Automobile Industry – Ducati Diavel, Activa, Tata, Mahindra Thar, Hyundai
Ducati Diavel 1260 Lamborghini Edition Unveiled: Limited To Just 630 Units For The World
Ducati Scrambler 1100 Pro and Scrambler 1100 Sport Pro Launched In India
Superbikes Manufacturer Ducati had announced that it will launch its Scrambler series in India. Luxury motorcycle brand Ducati today announced...
Latest News From Indian Automobile Industry – Honda Jazz, Audi RS Q8, MG Gloster, Nissan Magnite
Latest News From Indian Automobile Industry - Ducati Panigale V2, Honda Jazz, Honda Hornet, Audi RS Q8, Kawasaki Vulcan S,...
Ducati Panigale V2 Launched In India At Rs 16.99 Lakh – Indian Drives
Italian superbike manufacturer, Ducati has launched the Panigale V2 in the Indian market. The new Ducati Panigale V2 replaces the...
Ducati Multistrada V4 Coming In 2021 – Indian Drives
Ducati has revealed that it is currently working on Ducati Multistrada V4 and will be launching the same in 2021....
2019 Ducati Diavel 1260 and 1260S Launched in India
Ducati has launched the 2019 Diavel 1260 and 1260S in India at Rs.17.70 lakh and Rs.19.25 lakhs respectively. The new...
Ducati Panigale V4 25° Anniversario 916 Launched at Rs. 54.90 Lakhs
Ducati recently unveiled the Panigale V4 25° Anniversario 916 to celebrate the iconic 916's 25 years. The bike has now...
2019 Ducati Hypermotard 950 Launched In India At Rs 11.99 Lakh
The Ducati Hypermotard 950 in India has been launched at Rs.11.99 lakhs. In India, the bike will replace the Hypermotard...
Super Soco CUx Ducati Edition Revealed
Chinese electric two-wheeler maker Super Soco has launched a Ducati version of its CUx electric scooter. The scooter has been...
2019 Ducati Multistrada 1260 Enduro Unveiled
The 2019 Ducati Multistrada 1260 Enduro has been unveiled by Ducati. The Enduro version of the Multistrada 1260 comes with...
2018 Ducati 959 Panigale Corse Launched At Rs. 15.20 Lakhs
Ducati has launched the 959 Panigale Corse in India at Rs.15.20 lakhs. The bike, for now, will be available only...

redpajama_set_name: RedPajamaCommonCrawl


Welcome to Evolve Yoga + Wellness!
Evolve Yoga + Wellness is a community-oriented yoga and wellness center located in California, Maryland. Evolve welcomes many diverse styles of yoga as well as other mind/body and artistic modalities. We offer Barre, Tai Chi, Meditation, Massage Therapy, Pranassage and Reiki. We truly believe there is a type of yoga or movement for "every body", regardless of age, shape or flexibility.
In addition to group classes, we offer private sessions and consultations with wonderful wellness practitioners. Our practitioners specialize and are licensed in the areas of aesthetic services, skincare and energy work. We welcome local artists and musicians to exhibit their work and share their talents as well. Our goal is to create a dynamic and welcoming community in Southern Maryland. Our intention is to promote and enhance health, wellbeing and creativity on all levels.
Evolve is also recognized as a Registered Yoga School through the Yoga Alliance offering 200 and 300 hour yoga teacher training programs.


text:
http://www.barrons.com/articles/what-is-the-listless-market-telling-us-1477109949
What Is the Listless Market Telling Us?
Oct. 22, 2016 12:19 am ET
Reviewing the Listlessness
by Yardeni Research
yardeni.com
Oct. 19: Joe Abbott and I are seeing more articles speculating about either a meltdown or a meltup in the stock market after Nov. 8. We are inclined toward the latter, though a continuation of listlessness makes more sense. We are still aiming for 2300 to 2400 for the Standard & Poor's 500 next year, but there could be a prolonged period of wait-and-see after the elections. Let's make a list explaining the listlessness:
1) The Fed: The market might remain listless until the Fed hikes interest rates at the end of the year. That might be followed by a Santa Claus rally celebrating the Fed's one-and-done per year approach to normalizing monetary policy.
2) Economic fundamentals: The U.S. economy is likely to continue muddling along between a boom and a bust for the foreseeable future. The overseas economy is likely to do the same, though at a slower pace that may be better described as "secular stagnation."
3) Earnings: Joe and I believe that the earnings recession is over. S&P 500 operating earnings per share have declined on a year-over-year basis for the past four quarters through second-quarter 2016. Industry analysts are estimating it fell 0.9% during the third quarter. However, Joe and I expect the typical earnings season's upside "hook" as companies report actual results.
4) Valuation: As we discussed last week, there are no bargains in the stock market. Valuations are high. By definition, in a meltup, they certainly would go higher, but that would make the market vulnerable to a meltdown. Our bullish outlook for the market is based on our view that single-digit earnings growth will do most of the heavy lifting.
5) Sentiment: The Bull/Bear Ratio, compiled by Investors Intelligence, tends to be a good bullish contrarian indicator when it is at one or lower and bearish when it is three or higher. Its latest reading, as of Oct. 11, was two, indicating that sentiment is neither bullish nor bearish from a contrarian perspective. The ratio had jumped from this year's low of 0.63 during the week of Feb. 9 to the year's high of 2.81 during the weeks of Aug. 16 and Aug. 23.
6) Breadth. At the end of last year, the stock market's breadth, on the basis of the ratio of the equal-weighted to market-cap-weighted S&P 500 indexes, narrowed considerably. But just as this relative weakness was becoming a concern among technicians, the ratio rebounded 4.4%, from 1.505 on Jan. 19 to 1.571 through April 27. Since then, as the election approaches and the prospect of a Fed rate hike is nearing, the ratio has fallen 1.1% through Oct. 17. Nevertheless, the ratio remains near its record high of 1.597 during April 2015. Further, while only 28% of S&P 500 companies remain above their 50-day moving average as of Oct. 14, nearly 60% remain above their 200-DMA.
—Ed Yardeni
What Voters Are Liking
Current Market Update
by BMO Wealth Management
bmoprivatebank.com
Oct. 18: When asked, "What do you like about Donald Trump?" Kate McKinnon, playing Hillary Clinton on Saturday Night Live's presidential debate skit last Saturday, responded, "Donald Trump and I disagree on almost everything, but I do like how generous he is. Just last Friday, he handed me this election." The latest polls show Clinton breaking away from Trump leading up to this November's vote. PredictIt.org, a nonprofit trading site that lets participants "bet" on political outcomes, gives Clinton an 83% chance of winning the White House.
The investment markets concur. Since Sept. 26, the Mexican peso, a real-time indicator of Trump's political prospects, rallied 6.6% against the U.S. dollar, reversing a 13% slide that commenced last April. Meanwhile, biotech, Clinton's political piñata, has sagged versus the Nasdaq. Biotechs slid 8% relative to the Nasdaq since late September, reflecting Clinton's improving chances. Looking beyond the Oval Office, PredictIt.org suggest Republicans will lose control of the Senate. Their odds of maintaining a majority there are just 32%, although they should maintain their grip on the House. PredictIt suggests an 80% likelihood that the Republicans will maintain a majority there. And history suggests that investors prefer mixed government.
—Jack A. Ablin
House Buyers Face Tight Supply
Economic Update
by Regions Financial
regions.com
Oct. 19: Existing-home sales rose to 5.470 million units in September, falling between the consensus of 5.320 million units and our high-end forecast of 5.570 million. Inventories remain a persistent drag on sales, with the months-supply metric down to 4.5 months; this supports sturdy house-price appreciation, with the median sales price up 5.6% year on year. Reflecting lean inventories, average time on market was 39 days, down from 49 in September 2015. All in all, the current report is consistent with what for some time has been the housing-market narrative – solid demand-side fundamentals held back by supply constraints.
—Richard F. Moody
Sector Shifts in the S&P
Market Briefing
by Applied Global Macro Research
agmresearch.com
Oct. 18: We expect the S&P 500 to gain modestly over the next year, but the sectoral shifts could be significant. Banks remain the only sector in the U.S. that is appealing enough to warrant a recommendation. This is due to the combination of low valuations, exposure to housing/consumer low-credit risk, and immunity to rising rates and to rising labor-compensation pressures.
High-yield credit is probably the major asset class in the U.S. that is most attractively priced, but spreads have come in so much now, and the profit-margin cycle is so advanced, that we recently closed that recommendation and don't think this asset is overall attractive enough anymore.
We still recommend long positions in European and Japanese equities, as the digital manufacturing cycle is improving on the margin, but we will not be very ambitious with our profit targets for Europe.
We close our recommendations with global auto makers at a loss. This framework has not worked well in the past year; return signals are fading, and our U.S. and European consumer leading indicators are now less positive.
—Carsten Valgreen
The Money Is Still on Stocks
U.S. Investment Policy Committee Notes
by CFRA/S&P Global
cfraresearch.com
Oct. 19: The old rule of thumb was that the average person investing for retirement should have 100 minus their age allocated to equities. Now that we tend to live longer, that formula was upped to 110 minus your age. That said, a 41-year old planning to retire at 65 in 2040 would have about 70% exposure to equities. Yet today, the average 2040 target-date fund, according to CFRA mutual fund research, has an 80% equity allocation. What's more, the five largest funds have between 83% and 95% in stocks, averaging 88%. One likely reason investors believe that diversification didn't work in the last bear market was because they were overexposed to equities. Yet a 60/40 portfolio consisting of the S&P 500 and long Treasuries fell less in 2008 than it did in 1974.
—Sam Stovall
To be considered for this section, material, with the author's name and address, should be sent to MarketWatch@barrons.com.
Morning Briefing by Yardeni Research yardeni.


On the developer book you can find general info about how to work with launchpad and bazaar.
Regarding the right place to load your module and how the module has to be proposed, please read this announcement.
I have the same problem: where to put my module. I read your answer and your link but I don't understand how do to this. I don't want to post a new Question for the same problem but the documentation don't help me.
I want to create a module that create a SuperCalendar with holidays, task on project, phone meeting, meeting etc... What is the right place for that? It extends CRM, Project and maybe others in a near future.
I DL the server-env-tools for the v7.0 but all module's __openerp__.py file have parameter "installable" set to false. Is it an error? I set manually it to true but am I right? Another question: where can I discuss about this module?


text:
Defiant humor in 'Greetings from the Barricades: Revolutionary Postcards in Imperial Russia'
The 1905 Russian Revolution—which included worker strikes, mass peasant unrest and military mutinies leading up to the 1906 October Manifesto, in which Tsar Nicholas II was forced to concede basic civil rights and an elected parliament—preceded the Bolshevik Revolution by twelve years. During this time, revolutionaries began to use printed postcards as a cheap, effective conduit for their political ideas. This week, Four Corners Books has released Greetings from the Barricades, a beautifully designed and printed, 480-page hardcover collection of revolutionary postcards from Imperial Russia, compiled by Tobie Mathew. "Over recent years the internet has transformed the organization of subversive activity," Mathew writes. "Through Facebook, Twitter and YouTube, opposition parties and terrorist groups have acquired instant access to citizens the world over. A hundred years ago the Russian revolutionaries were not so very different from today's militants and freedom fighters—a small band of committed individuals who needed to convince a nation to act against what they perceived to be a morally bankrupt regime. The medium they used may have been less technologically advanced, but it was no less effective in communicating partisan tales of popular resistance." Featured image, a hand-drawn caricature of Tsar Nicholas (c. 1905) which appears in the book and comes blown-in as a beautiful stand-alone postcard, is entitled "Engrossed in Reading," after Georgii Erastov.
Greetings from the Barricades
FOUR CORNERS BOOKS
Hbk, 6.75 x 9.75 in. / 480 pgs / 160 color / 60 b&w.


text:
Global Opinions
The Opinions Essay
D.C., Md. & Va. Opinions
Cape Up
Post Opinión
Amy Coney Barrett's judicial record should alarm liberals
U.S. Court of Appeals for the 7th Circuit Judge Amy Coney Barrett, a law professor at the University of Notre Dame. (Matt Cashore/Notre Dame/Via Reuters)
Opinion by
Ruth Marcus
Deputy editorial page editor overseeing signed opinion content and writing on domestic politics and policy
Deputy editorial page editor
September 20, 2020 at 10:46 p.m. UTC
When President Trump was down to the wire in naming a replacement for retiring Supreme Court Justice Anthony M. Kennedy, one of the strikes against federal appeals court Judge Amy Coney Barrett was her scanty judicial record.
Conservatives had learned a painful lesson with previous picks — Justices Sandra Day O'Connor and David Souter — who turned out to be more moderate than advertised. They had internalized the experience: No more stealth nominees. Candidates needed to have a lengthy enough judicial paper trail to be confident of how they would perform on the high court.
So Barrett, named to the U.S. Court of Appeals for the 7th Circuit just eight months earlier, lost out to Brett M. Kavanaugh — even though an examination of her academic writings strongly suggested that, at least on the issue most important to social conservatives, she would be solidly opposed to abortion rights and inclined, even eager, to reverse Roe v. Wade. As I wrote at the time, "while Barrett has the shortest judicial paper trail of the likely nominees, her academic writings are the equivalent of a flashing neon sign: I'll do it."
More than two years later, Barrett has amassed a judicial track record — nearly 100 written opinions, and many more votes on cases before her — to support that assessment. In her still relatively short time on the bench, Barrett has considered two abortion cases and ruled against abortion rights in both.
Live updates on Ruth Bader Ginsburg's death
In one, the full appeals court declined to review a panel decision that blocked from taking effect an Indiana parental-consent law for minors seeking abortions. The law on this has been fairly clear, for decades: It is constitutional for states to require that minors seeking abortions obtain parental consent. However, such laws must provide what is known as a judicial bypass, allowing the minor to demonstrate that she is mature enough to make the decision on her own or that an abortion would be in her best interest.
Amy Coney Barrett is rumored to be one of the leading names on President Trump's shortlist of potential Supreme Court justices. Here's why she's controversial. (The Washington Post)
Notwithstanding this settled law, Indiana enacted a parental-consent law that mandated that the parent be informed of the planned abortion unless the judge further decided that it would not be in the minor's "best interests." A district judge blocked the law, and a three-judge appeals court panel agreed. The panel, splitting two to one, noted the "serious risk that prior notice, instead of giving parents an opportunity to offer wise counsel, will actually give parents an opportunity to exercise a practical veto, preventing the pregnant minor from actually exercising the constitutional right the juvenile court has allowed her to exercise."
The full appeals court, dividing six to five, let that decision stand. Barrett and two other Trump nominees joined the dissent, which stated the issue as a matter of federalism: "Preventing a state statute from taking effect is a judicial act of extraordinary gravity in our federal structure."
The second case involved an even more extreme Indiana law, signed by Vice President Pence when he was governor: It prohibited abortions performed for reasons related to sex, race or disability. Specifically, a woman who discovered that her fetus had Down syndrome would be barred from terminating the pregnancy.
An appeals court panel composed of three Republican appointees agreed with the lower court that the law was flatly unconstitutional. "The non-discrimination provisions clearly violate well-established Supreme Court precedent holding that a woman may terminate her pregnancy prior to viability, and that the State may not prohibit a woman from exercising that right for any reason," the court said.
It rejected Indiana's argument that the right to abortion protected under Roe included only the decision whether or not to bear a child, not whether to continue a particular pregnancy. "Nothing in Roe … or any other case from the Supreme Court can be read to limit a woman's right in this way," the court said.
Indiana didn't ask the appeals court to reconsider that part of the ruling, just a different aspect of the law involving the disposal of fetal remains. That didn't stop Barrett from joining a dissent that labeled the law a "eugenics statute." The opinion, issued just before Kennedy announced his retirement, argued that "none of the Court's abortion decisions holds that states are powerless to prevent abortions designed to choose the sex, race, and other attributes of children." Talk about judicial activism — the question wasn't even before the court.
Of course, there is much more to constitutional interpretation and judicial philosophy than abortion. To take one other hot-button example, in 2018, gun rights groups were concerned about Barrett's blank slate on the issue. Now they have before them a 2019 case involving a Wisconsin man, convicted of felony mail fraud, who claimed that federal and state laws prohibiting felons from possessing firearms went too far in his case, without any indication that he posed a danger. Two Republican appointees upheld the laws. Barrett dissented, saying that denying arms to all nonviolent felons treats the Second Amendment as a "second-class right."
Barrett dissented in a case in which the majority blocked the Trump administration's "public charge" rule, which excludes the entry of legal immigrants who might rely on federal benefits. She joined a ruling that job applicants cannot use age-discrimination law to sue over hiring practices that have a discriminatory impact on older workers.
On the other hand, she found that a male butcher who was subjected to harassment and unwanted touching by male co-workers could sue under federal anti-discrimination law. "The shop was a mixed-sex workplace, and only men were groped and taunted," Barrett wrote. "Because men were treated differently from women at [the store], a reasonable jury could conclude that [the plaintiff] was tormented because of his sex."
There is much more to plumb in Barrett's writings, as Trump weighs his selection. But a quick review suggests that conservatives should be assuaged, and liberals alarmed, by the Barrett record in her first years as a judge.
From Bernice King to Sheryl Sandberg, these are the stories of women inspired to exercise their most fundamental democratic right by those who voted first. (The Washington Post)
Jennifer Rubin: Justice Ginsburg is gone, but democracy must survive
Karen Tumulty: Senate Republicans are showing us why they should lose their majority
Goodwin Liu: Ginsburg's vision led us to a better America. We can do the same.
The Post's View: Ruth Bader Ginsburg spent her life fighting double standards. Republicans should not embrace one to replace her.
David French: Trump picked the wrong judge
Ruth Marcus: The Trump Supreme Court pick who'd pose the biggest danger to abortion rights
Ruth Bader Ginsburg's death and succession
The justice's passing opens up a battle for her replacement
The latest: Trump nominates Amy Coney Barrett to fill Ginsburg seat | Amy Coney Barrett, a disciple of Justice Scalia, is poised to push the Supreme Court further right | Tumultuous path to sixth conservative justice puts Supreme Court in the middle of political fray | Who is Amy Coney Barrett? | What's next in the Supreme Court confirmation process for Amy Coney Barrett | Where GOP senators stand on quickly filling Ginsburg's Supreme Court seat
Photos: The life of Ruth Bader Ginsburg | Crowds gather at Supreme Court to mourn the justice
Complete coverage: Justice Ruth Bader Ginsburg dies at 87


text:
Melbourne at war
Travelling Well | Mike Rosel | Posted on 07 November 2017
The forgotten story of civilian Australia's World War II experience.
When young archaeologist Barry Green and his wife and fellow archaeologist Alana investigated a building site at the Royal Victorian Institute for the Blind in St Kilda Road in 2014, they hoped to unearth a 19th-century fever hospital.
But the excavation yielded evidence of a condition just as alarming: the invasion fear that dominated Australian life for most of 1942.
The pair found the unmistakable outline of a WWII air-raid trench, its zig-zag pattern intended to limit blast damage. This one had an unusual horseshoe design which Barry surmises might have been for area defence of the RAAF and naval units that served here.
Wartime photographs look down on original leather chairs and radiators.
While their nearby digs had turned up 19th-century relics including clay pipes, bottles and broken plates marked Victorian Asylum & School for the Blind, their cross-sections of the trench found nothing.
Recalling how archaeologists sought 'crop marks' on early aerial photographs for indications of vanished structures, Barry searched photographs of 1945 without seeing his trench outline. He eventually found his ghosts in the grass on Google Earth images.
Other ghosts of this unsettling period – prime ministers Menzies and Curtin, US General Douglas MacArthur and more – were easily conjured up when RoyalAuto visited the well-preserved War Cabinet Room at Victoria Barracks in St Kilda Road where Australia's war was managed from 1939 to 1945. Wartime photographs look down on original leather chairs and radiators, blackout curtains, roller maps of empires now dust, a map board easily concealed by lockable panels and a black rotary-dial telephone.
Our guide waved a brass ashtray: "Everybody smoked cigarettes, pipes or cigars… sometimes sessions lasted 18 hours … they installed fans above the door to suck the worst of the smoke into the typing pool." It's regrettable that the barracks were closed to public tours following the 2009 terrorist plot aimed at Holsworthy Army Barracks outside Sydney.
Irish-born Barry Green, who emigrated to Melbourne in 2009 with his Australian wife, had done a crash course in our wartime history, and was startled to discover how little younger generations knew of the near hysteria that followed Japan's surprise attack on Pearl Harbour on 7 December 1941, and Japan's military advance across South-East Asia.
Australia was a nation living in fear during 1942.
"I was surprised to find how quickly the civilian experience of the war had been forgotten, including the pivotal role Melbourne played," he says.
His reading included On The Home Front: Melbourne in Wartime 1939-1945, by historian Professor Kate Darian-Smith from Melbourne University. Prominent buildings were sandbagged or partly bricked up; thousands of volunteer air-raid wardens tried to enforce a blackout; some scared families departed for distant refuges; key museum treasures were removed for safe keeping. There was heavy censorship, rationing and no private petrol.
"There were hundreds of slit trenches," Barry says.
"Almost two kilometres of trenches around the city alone, notably in Treasury Gardens outside State Government offices, with uncounted others in municipal parks, schools and institutions, and backyards." These were not the coffin-deep narrow slits you might imagine: a regulation trench was only 1.22 metres deep and a metre wide at the top, built shallow to reduce the chance of walls toppling.
Kate noted that "civilian morale plunged to an unprecedented low" after military disasters.
"Australia was a nation living in fear during 1942, as was clear in my interviews with more than 100 people who endured the wartime city," she says.
"The separation of families, the nightly blackout and air-raid drills, and the constant uncertainty about the future contributed to feelings of stress and heightened emotions."
Human nature often conflicted with the Anzac spirit.
This was a spirit-sapping rollercoaster. Australians were stunned by Singapore's fall on 15 February 1942 (with some 15,000 Australian soldiers captured) and the first bombing of Darwin on 19 February, with around 300 deaths.
Rumours flourished. For instance, some people had claimed to see a small Japanese floatplane over Melbourne early on 26 February. This rumour turned out to be true, if not officially acknowledged until 1945.
It was 50 years before author David Jenkins tracked down pilot Nobuo Fujita, and Australians learned how his plane had been taken from a hangar on the deck of submarine I-25 off King Island in Bass Strait. Fujita took off in the dark for his audacious dawn patrol.
While fears eased after American carrier-borne aircraft won the Battle of the Coral Sea in early May, morale took another hit when three Japanese midget submarines penetrated Sydney Harbour later that month.
Spirits soared with the sinking of four Japanese aircraft carriers in the pivotal Battle of Midway in June – and fell as the Japanese advanced towards Port Moresby along the Kokoda Track, soon infamous for jungle warfare that ebbed and flowed until the final enemy retreat in November.
Melbourne breathed again. Trenches became playgrounds for kids such as Noel Carrick, who remembers trenches off High Street, Malvern, as "stinky and grungy" after rain. Some people, focused on moral rather than military welfare, complained that trenches provided privacy for lovers.
Painter Albert Tucker's bleak vision of Melbourne's dark side emerged in his Images of Modern Evil series.
The city was invaded, of course, when the 1st US Marine Division arrived from Guadalcanal in January 1943. Melburnians welcomed the American build-up, excepting those men who complained about their competition as "overpaid, oversexed and over here". Citizens were shaken by the 'Brownout Murders', when a serial killer throttled three women in May; the arrest of US Marine Edward Leonski did little for Australian-US relations.
Kate investigated recruitment of women for munitions factories and other workplaces, and social and sexual upheavals. While volunteering was popular – from air-aid precautions to "knitting circles for the troops" – human nature often conflicted with the Anzac spirit. The black market thrived, black American troops were not always welcomed, and some unions resisted the women who replaced workmen serving in the Forces. Painter Albert Tucker's bleak vision of Melbourne's dark side emerged in his Images of Modern Evil series.
Barry Green says he will be spending time "trying to shed more light on Melbourne's forgotten military landscape".
Images: Australian War Memorial


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Home » Poverty Measurement: Guide to data disaggregation adopted by UNECE
Poverty Measurement: Guide to data disaggregation adopted by UNECE
The United Nations Economic Commission for Europe (UNECE) has adopted a Guide to Poverty Measurement and data disaggregation which is now formally endorsed by the Conference of European Statisticians (CES). The CES sets international statistical norms and standards for use in 60 European and other countries. The purpose of the Guide is to provide methodological and practical guidance on poverty disaggregation in order to enhance further international harmonisation. It includes references to the UK Poverty and Social Exclusion (PSE) projects and subsequent work (see especially Chapter 5).
The Task Force which developed the guide included the National Statistical Offices of Austria, Canada, Czechia, Italy, Mexico, Slovakia, Russian Federation, Switzerland, the United Kingdom and the United States of America. Professor David Gordon was asked by Statistics Austria to suggest a recommendation on deprivation measures - which was adopted at the United Nations Economic and Social Council Sixty-eighth plenary session in Geneva on 22–24 June 2020.
Recommendation 28 draws from our work on the methodology for determining deprivation measures for the European Union:
a) Deprivation measures need to be based upon a clear and explicit theory or normative definition of poverty in order to ensure that each indicator is a valid measure, i.e. that it measures poverty and not some other related (or unrelated) concept such as wellbeing or happiness.
b) The validity of each indicator should be demonstrated, i.e. the amount of systematic error should be formally assessed and indicators should be dropped if they have a low validity.
c) The reliability of each indicator should be determined, i.e. the amount of random error should be formally assessed and indicators should be dropped if they have a low reliability.
d) A deprivation or poverty index should only ever be weighted if this results in a reduction in measurement error, i.e. if the differential weights improve the validity and/or reliability of the index.
Other Recommendations that might be of interest include Recommendation 29 on child poverty:
a) Countries should use available datasets, such as Multiple Indicator Cluster Surveys (MICS) or household surveys to develop child-specific and life-cycle adapted multidimensional poverty measures that reflect the needs of children at different stages of development and allow for identification of intra-household differences between children. This type of measure can be performed at intervals of 3-5 years to complement more frequent disaggregated national measures, as this will give greater insight into childhood and adolescent poverty.
b) In order to enhance availability and use of child poverty data, countries should collect data on all key dimensions related to children's rights, including health and nutrition, and introduce lifecycle appropriate indicators to measure the situation of each child in the household. Countries should consider introducing innovative ways to collect, monitor and report on child poverty data, including ways to encourage child participation in the monitoring and discussion of child poverty data and potential policy responses.
c) In accordance with national definitions of monetary and multidimensional poverty, countries should revise and adopt survey tools to best serve their national needs for poverty measurements. Both household budget surveys (HBS) and MICS are flexible and can be adapted to reflect a national context, but without compromising cross-country comparability. MICS offers the potential to obtain data on a broader list of child-focused indicators that can be used to measure multidimensional child poverty.
d) Statistical data is an important source for evidence-based decision making by policy makers, not only at national but also at regional and international level. Therefore, it is important to make anonymised statistical data openly available for all users. To meet data protection and confidentiality concerns, efforts must be taken to ensure that the identity of respondents is not disclosed or can be inferred. Hence countries should make all poverty-related data, including micro-data, publicly available and easily accessible for scientific research and production purposes. This would enhance research, policy design and policy innovation in this field, which is of utmost importance for devising policies for poverty reduction.
Recommendation 26 on intrahousehold poverty measurement may also be of interest:
a) In the immediate term, official poverty rates, collected at the household level, should be routinely disaggregated by sex and age of each household member. This shall provide estimates for the poverty rate of prime age women who have children and/or live without a partner (e.g. in lone parent households).
b) More research is needed to determine how best to address intra-household resource sharing in order to develop sub-household measures of poverty status. This is particularly important for the disaggregation of poverty estimates by sex and age. Surveys should continue to experiment with questions designed to determine individual control of resources and to measure material deprivation at the person level.
c) Where possible, official poverty rates for men, women, children or other socio-demographic subgroups should be accompanied by results that consider unequal sharing of resources. At a minimum, national statistical offices should carry out sensitivity analysis for poverty profiles contrasting the conventional full pooling assumption with partial pooling and full separation of resources.
d) To validate assumptions on within-household distribution of economic resources, these should be considered in combination with material living standards, wherever possible. Questions on sharing of personal economic resources and/or personal material living standard have been used in EU–SILC. Before such questions are adapted it should however be ensured by pre-tests that sharing of resources is not considered as sensitive by respondents.
You can also find further details on the consultation outcome in the CES Summary note. An updated paper copy of the electronic Guide will be published by the end of the year.
NOTE: the first UN Handbook on Poverty Statistics was published in 2005, it primarily focused on rather narrow definitions of monetary poverty measurement from a mainly econometric perspective. In 2006, the Compendium of Best Practices in Poverty Measurement was published by the United Nations Expert Group on Poverty Statistics (Rio Group). This Compendium involved poverty experts from both National Statistics Offices and academia from 22 countries and 18 regional or international organizations, between 1996 and 2006, and provided a much broader perspective on poverty measurement. A number of UN Regional Organizations, such as UNECE, have subsequently published recommendations on poverty measurement which include recent technical developments and theoretical advances in poverty measurement.
Low-income households
Poverty forecast


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Good Things Foundation - a social change charity, helping people to improve their lives through digital.
Online Centres Network - a network of community partners who help people improve their lives through digital.
Learn My Way - a website of free online courses for beginners, helping people develop their digital skills.
Good Things Foundation Australia - our Australian website.
Be Connected - an Australia-wide initiative empowering all Australians to thrive in a digital world.
English My Way - a website of resources for tutors who support and teach adults with no or low levels of English.
Learn My Way needs JavaScript to work properly. Please enable this in your browser settings before using this site.
Bridging the Digital Divide
Motivational barriers
New year, new government: The outlook for Good Things Foundation and the Online Centres Network
14 Jan 2020 |Written by Sam Green
New year, new Government. Boris Johnson found success in breaking the Labour Party's monopoly in many of the northern constituencies, helping the Conservative Party to enter the new decade with a landslide parliamentary majority.
His primary concern will be to deliver on the Conservative's election slogan and 'get Brexit done' by 31 January 2020, and whilst the Withdrawal Agreement still leaves much of the future UK-EU relationship to be negotiated, it might well signal the end of the beginning.
This will allow the focus to shift on to domestic policy. The Government will be keen to retain the support of their new constituencies, many of which voted Conservative for the first time. With the Chancellor declaring an end to austerity, there may be good news ahead for the community sector.
Here is what we can expect to see over the course of the next Parliament in the key policy areas for Good Things Foundation and the Online Centres Network.
Digital skills, inclusion and further learning
The Conservatives have pledged to cover the UK with 'gigabit-capable' broadband services by 2025, spending £5bn to support provision in the 20% hardest to reach areas.
Access to the internet clearly relies on broadband coverage - but even with faster pipes, there will still be people who won't be able to use it. Alongside investment in infrastructure, we need investment in skills so that everyone is able to access the benefits the internet has to offer.
A new £3bn National Skills Fund has been announced as a step towards what the Conservatives have called the 'Right to Retrain' for all adults. Their manifesto pledged to 'invest in Britain's people by giving them the tools and training to flourish in the economy of the 21st century'. In an election which saw cross-party consensus that there is a skills gap that needs addressing, it's likely that this will be a policy area where the Government will be keen to make a mark.
Since there are 4.1 million adults who have never been online in the UK, and a staggering 11.9 million people who lack Essential Digital Skills, we will be working with the Government to ensure that digital skills remain a priority, and that the Online Centres Network continues to play an important role in provision. Through our Future Digital Inclusion programme funded by the Department for Education, we've helped more than 3 million people learn basic digital skills since 2014.
The NHS was a key focus of the election campaign, with all parties battling it out to be seen as champions of the health service. Brexit aside, this is likely to be the Government's main priority, and early legislation will give the NHS a £33.9 billion increase by 2023-24.
Matt Hancock has returned to his role as Secretary of State for Health and Social Care. With previous experience as both Digital Minister and Skills Minister, the Secretary of State is a strong advocate for digital. NHSX, the digital arm of the health service, was launched early last year.
We can expect to see the Government ramp up the digitisation of health services and deliver on the NHS Long Term Plan, with digital-first primary care becoming a new option for patients. Appointments and prescriptions will continue to be digitised and the NHS App will be developed to create a digital NHS 'front door'.
Of course, people can only reap the benefits of a digitised health tools if they have the confidence and capabilities to use them. Working with the NHS, we have been developing more than 20 pathfinders that model ways to engage and support the most excluded groups across England.
One of the first pathfinder projects in Sheffield involved supporting people with long-term conditions such as diabetes and asthma to use digital tools to improve the management of their health conditions. We will continue to champion the role of community organisations in reducing health inequalities, and in working with the more formal health service within communities.
Online harms
Harmful content - including disinformation (or 'fake news') and extremist propaganda - has exploded with the rise of social media. In the Queen's speech, the Government confirmed that making the UK the safest place in the world to be online will be a priority.
Legislation will be shaped by the recommendations of the Online Harms White Paper, which was published in April 2019 and received cross-party support. It calls for the establishment of a new statutory duty of care for companies to take more responsibility for their users' online safety, and the creation of a new regulator to enforce it.
Through our online safety course on Learn My Way, our learning platform, we help people to be safe online. Of the 4.1 million people who have never used the internet, 60% say that they are offline because they're worried about their identity being taken. The hyper-local organisations in the Online Centres Network know their communities very well, and can offer face-to-face support to help people gain the confidence they need to overcome fears of encountering online harms.
At Good Things Foundation, we'll continue to work closely with our partners across the political spectrum and in a range of departments to ensure we can continue to support those who are digitally and socially excluded, as well as the community organisations in the Online Centres Network who are on the frontline of providing this crucial support.
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Shadow of the Colossus – PlayStation 2 Retro Review
By Jake Lawler
on October 24, 2016 2 min read
Available Elsewhere?
PS3, PS4
Approx Value?
£5+
Anyone who played Shadow of the Colossus, whether it was the HD PlayStation 3 remaster or the original 2005 release had the call "Argo" burned in their brain.
Released by Sony, it was arguably the most visually stunning PlayStation 2 game ever created, well at least it was for me.
The plot of the game has always been somewhat vague due to the extreme lack of dialogue. It's a fantasy world taking place in a 'Forbidden Land' surrounded by sea, canyons, caves and even the ruins of man-made structures.
You play as 'Wander' a young man who is tasked with resurrecting a mysterious girl. To do that you must slay 16 Colossi (easier said than done) who all live in different environments with different weaknesses. You must constantly be adapting to survive.
To do that you must slay 16 colossi (easier said than done) who all live in different environments with different weaknesses. You must constantly be adapting to survive.
Jumping and clinging to the fur and different ornaments spread around the body of a Colossi is one of the most awe-inspiring video game moments. The incomprehensible scale of the beasts has never since been captured virtually.
The fluidity and movement in Shadow of the Colossus is special in its own way and was critical in the feel and emersion of the game.
Argo (The trusty horse companion for those who don't know) was a big help in getting around the environment and the large open spaces, which somehow still always felt full, despite the vastness.
Some battles heavily relied on Argo, and some took place entirely on water, rendering Argo useless!
Once you start down the path, you won't stop raising your sword to the sky trying to pinpoint where the next battleground is, well not until you've taken down all 16. Each of the battles feels new and different, no repetitive gameplay here.
Many consider this just as much as a puzzle game as an Action adventure game. You have to be able to find and exploit a variety of different weaknesses, or there is absolutely no chance you are going to be triumphant. The grip mechanic is unique and requires an extra level of attention if you want to stay perched on top or clinging to the monster. If you fail and let the meter completely diminish you risk falling and losing your advantage over the colossus.
The grip mechanic is unique and requires an extra level of attention if you want to stay perched on top or clinging to the monster. If you fail and let the meter completely diminish you risk falling and losing your advantage over the colossus.
I can see how fans of many genres can come together and appreciate this… work of art. It provides Puzzles, action, adventure, collecting and leveling up.
And to be honest, who doesn't want to fight beasts 100x larger than your character and actual feel like it was a fair fight that you deserved to win.
All in all if you remember Shadow of the Colossus you should really play it again and if you never have, it's one to add to your must play list.
Is it worth playing again?
A game of immense beauty that deserves your attention. Go grab your PS2 out of the loft or get this game on eBay and prepare to be amazed at its desolate splendor.
Classic Factor
Reader Rating2 Votes
Good Bits
Beautiful game to look and play
Bad Bits
Plot is a bit vague
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Klistron refleksowy  – generacyjna lampa mikrofalowa, posiadająca w odróżnieniu od klistronu dwuobwodowego jeden rezonator.

Elektrony po opuszczeniu wyrzutni przelatują przez szczelinę rezonatora, następnie są zawracane z powrotem do tej szczeliny za pomocą elektrody spolaryzowanej ujemnie (względem katody), zwanej reflektorem. Również w tym typie klistronu elektrony poruszając się z powrotem w kierunku rezonatora grupują się – elektrony szybsze doganiają wolniejsze powracając do szczeliny "paczkami", a nie jako jeden ciągły strumień. Sprawność klistronów refleksowych jest niewielka i nie przekracza kilku procent. Mają one zastosowanie w odbiornikach mikrofalowych jako generatory heterodynowe oraz jako źródła mocy w generatorach pomiarowych.

Zobacz też
 klistron
 magnetron

Bibliografia
 Hanna Górkiewicz-Galwas, Bogdan Galwas Przyrządy elektronowe, Wydawnictwa Szkolne i Pedagogiczne, Wydanie IV poprawione, Warszawa 1986

Linki zewnętrzne
 Aleksander Zawada Doświadczalny Tor Mikrofalowy (artykuł na stronie www.pwl.mikrokontroler.pl)

Lampy elektronowe
Technika mikrofalowa

redpajama_set_name: RedPajamaWikipedia


Our 10′ x 10′ Popup tents are the perfect for small parties, carnival games or concessions. They are inexpensive and can be setup and taken down in minutes. Each 10′ x 10′ tent has enough space for 2 of our 6′ tables and 12 chairs.
ALL TENTS must be at least 20′ in all directions from the nearest overhead utility lines.
Don't forget to add an inflatable, a concession machine, an outdoor game, or some audio or video equipment.


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De Lalande kan syfta på:
Joseph Jérôme Lefrançois de Lalande, astronom, Frankrike
Jean de Lalande
Marie-Jeanne de Lalande
Michel Richard Delalande

Se även
De Lalande – en krater på Venus, se Lista över kratrar på Venus


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Netmusiczone Records (auch: NetMusicZone Records) ist ein Independent-Label aus Bad Hindelang im Allgäu und eine hundertprozentige Tochter der Brainstorm Music Marketing AG. Unter Vertrag stehen deutsche und internationale Künstler, vornehmlich aus den Bereichen Rock und Alternative.

Angeschlossen an das Label sind ein Künstler-Management und seit 2015 eine Inhouse-Booking-Agentur. So übernahm man das Exklusiv-Management für Künstler wie Femme Schmidt, Equilibrium und Accept und arbeitet im Live-Bereich unter anderem mit Henning Wehland und der südafrikanischen Band Prime Circle zusammen.

Künstler
 The Stories
 The New Roses
 Marrok
 Black Space Riders
 Skull Fist
 Bloodpit
 Die Elenden
 Tiger Tunes
 Rising Girl
 Mark Reeder
 Anne Clark
 Klaxons
 Geist
 Who Killed Bruce Lee

Weblinks
 Netmusiczone Records bei Discogs
 Offizielle Webseite

Einzelnachweise

Independent-Label
Deutsches Musiklabel
Unternehmen (Landkreis Oberallgäu)
Bad Hindelang


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Берковець Володимир Семенович, (22.04.1941-15.11.2008). Народився в Носівці. Випускник Носівської середньої школи №1. Закінчив КПІ, працював в Інституті радіоелектроніки (НДІ "Квант") Головним конструктором. Опублікував близько 50-ти робіт з обчислювальної техніки. Почесний винахідник СРСР. Його винаходи і розробки впроваджені у різноманітних системах озброєння, що їх використовують армії України, Росії та інших держав світу.

Посилання

Джерело
 Фурса В. М. «Славні імена Носівщини». — Ніжин : ТОВ "Видавництво «Аспект-Поліграф», 2009. — 200 с. : іл. ISBN 978-966-340-357-1

Персоналії за алфавітом
Уродженці Носівки
Народились 1941
Померли 2008
Винахідники XX століття
Українські винахідники


I have been living here in Finland for close to 7 years now, after coming to Finland in 2011 in search of new adventures. I fell in love with the arctic and a local Finnish woman and have never left. While Enontekiö and Kilpisjärvi are my home and base for my guiding business, I have been lucky enough to live and visit a large number of places throughout Finland. Below is a summary of my Finland, in 5 photos. Enjoy!
These are the fells of Pallas-Yllästunturi National Park in the middle of autumn. This was taken the old fashioned way, out the window of a 2 seater aeroplane, piloted by my wife's Uncle. The park has everything Lapland has to offer in one location, open fell tops, forests, marshes and lakes. As one of the national parks certified guides it was great to be able to see one of my workplaces from the air.
Kilpisjärvi, located in the arm of Finland, on the border of Sweden and Norway, is my home. There is nowhere else in Finland which offers the same mountainous landscapes. It's a fantastic place for viewing the northern lights, and in winter you can ski or snowshoe pretty much anywhere you like. This shot is taken under Saana Fell looking over Lake Kilpisjärvi towards the Norwegian mountains.
At the other end of the country is Teijo National Park. It's only a couple of hours from Helsinki, close to Turku and has around 80km of hiking trails. I was sleeping in of the laavu's (a lean-to-shelter) in the park and was woken by the sun at around 4:30am to find myself shrouded in mist. This was one of the last photos I shot before the mist cleared. Misty mornings are common in Finland, particularly in autumn as the temperatures start to cool.
For me, this shot is winter. It's one of the reasons I never went back to NZ. The temperature at the time was -42 C, the air was crisp and froze on the back of my camera every time I took a breath. When I looked through the viewfinder, my nose would freeze to the screen. Both our cars wouldn't start and while most people stayed indoors, I was out exploring on snowshoes for a good couple of hours. I may not have been born in the north but I often feel as if I was meant to be.
I also love forests, which is a good thing as Finland is a land of forests, with seventy five percent of the country covered by them. In the middle of summer, when everything is lush and green, that's when they are at their best. This image was shot at Koli National Park back in 2015. The views from the top of the of the park are amazing, but it was the lushness of the forest which stood out for me.


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Yes, money matters
SAJJAD BAZAZ
Publish Date: Jul 1 2019 3:19AM
Updated Date: Jul 1 2019 3:19AM
Let me start this newly assigned column with two things about money - fact and truth. All of us have been taught about the importance of money and the fact that money brings us happiness. Money certainly affects our level of happiness. If we are having enough money, we are satisfied from the financial perspective of our lives. But the truth is that money cannot buy contentment.
Leaving the fact and truth aspects of money aside, it's important to take control of your money. This way, you would be taking control of your life, too. Of course, money is not everything in life but it is part and parcel of our lives. For achieving financial prosperity, its important to keep your money in circulation, allow it to change hands and get it multiplied through investment and savings schemes.
When we talk of investment and saving schemes, we have to be very careful in terms of the safety of our money. We have two environments, regulated and unregulated, where schemes are available to multiply our money. Regulated environment is the safest zone where money can be invested in schemes which are regulated by the regulators like the Reserve Bank of India, Securities Exchange Board of India (SEBI) etc. In an unregulated zone, there are financial schemes which offer higher returns on investment. But here the money is not safe and investors are at risk to lose even their capital investment.
These unregulated schemes are mostly driven by Ponzi schemes. In a Ponzi scheme, investors are paid from money collected from new investors instead of the scheme's earnings. The scheme runs as long as new investors keep investing in the scheme and actually yields the promised returns to earlier investors, as long as there are more new investors. But collapse when the new investments stop.
Precisely, when the Ponzi scheme stops giving the returns to the investor, it proves as a Ponzi trap and leaves the investors devastated. These are the schemes which feed on greed and are designed innovatively in such a way that they trigger endless greed in people. This greed lures them to invest in these schemes without giving a thought to the risk of losing the money.
The irony is that locally as well as globally well-educated people fall into the infallible trap of Ponzi schemes. People are so blinded by the seemingly incredible returns that they seldom think how they could possibly earn such high interest on their investments.
In the past few years, tens of thousands of UAE residents have lost their life savings in investment plans only to discover that these were outright Ponzi schemes.
Let me reproduce one such global ponzi trap where nearly 6,000 residents lost their money invested in Sunfeast Infotech. At this company, investors looking to make extra bucks from 'outsourced projects' were handed a flash drive with several pages of manuscript in PDF format which they were required to type into text format and submit within 25 days.
At the end of a 30-day cycle, they were paid Dh250 for the job. They had to pay a security deposit of Dh500 for each project. In theory, they got their initial investment in two months; any extra job after that was profit.
Enticed by big returns, thousands used to queue up at Sunfeast's office during 2013 with many taking huge loans to procure hundreds of 'projects' at the same time.
When that was not enough, scores sold their jewellery and homes. One enterprising man even set up a temporary typing centre at his home in India where young students were hired to do the job.
Nobody bothered to find out how anyone could make a fortune out of typing a few sheets of paper. By the time the company was shut down by the Dubai Economic Department (DED) and its owners jailed for fraud, millions had been siphoned off.
Back home in India, I Monetory Advisory (IMA) Jewels ponzi scheme fraud is the latest one which surfaced recently. If media reports are to be believed, the size of the scam is about Rs.5,000 crore, with more than 30,000 people cheated by the ponzi scheme company. The owner of the company has already fled out of the country. People not only from Bengaluru and Karnataka, but also from Hyderabad, neighbouring Tamil Nadu and New Delhi have invested in the company.
The modus operandi of this 13-year-old company was to lure Muslim investors in the name of Shariah investment. The investors were told that they won't be getting interest, which Islam doesn't encourage, but would be getting profits.
So, the company made them to invest by telling them they were partners. It gave out profits which amounted to at least to 3 per cent a month (or 36 per cent annually), which is much higher than the rates given by banks on fixed deposits.
South Indian states have a history of such so called Halal Ponzi schemes where the companies like IMA Jewels, Heera Gold, Burraq etc have fooled vulnerable investors in the past many years by taking advantage of their religious beliefs. They offered investment schemes to be compliant with the Islamic law of Shariah, but ultimately duped the investors of their hard earned money.
Interestingly, Heera Gold Group, which later proved a Ponzi company, had sponsored a cricket tournament in the UAE and recently had announced Rs 10 million aid for Kerala flood victims. Who would have thought all this was a façade. The investors had even no reason to suspect anything amiss as the company gave them monthly returns.
Now the main question: How to protect against such Ponzi traps? The mantra is simple. If anyone is considering investing in a scheme that they've been advised or even promised will give them very high returns -- it's probably best to avoid it because it may well be a scam. A rule of thumb of the financial market is: "What seems too good to be true, is never true. There is no other interpretation of this evergreen cliche."


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Shapeshifters VS Rachel Stevens - Chart Battle!
Tuesday, August 1, 2006 - 07:24
There's a battle on for Sunday's singles chart top spot, between Shapeshifters and Rachel Stevens.
In the Ibiza anthem corner is Shapeshifters' 'Lola's Theme'; while Rachel Stevens rocks the fit electro pop corner with 'Some Girls'.
At present, Shapeshifters are ahead by a nose but there's still lots of time for Rachel's Richard X-crafted track " the official single for Sports Relief.
Also heading for top five entries are Morrissey's 'First Of The Gang To Die' and Jamelia's Chris Martin-penned 'See It In A Boy's Eyes'.
J-Kwon's 'Tipsy' and Marillion's 'Don't Hurt Yourself' both look set to enter inside the top ten.
More From Rachel Stevens
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Rachel Stevens Named FHM's Sexiest Woman Of All Time
Rachel Stevens Gives Birth To Second Child
Rachel Stevens Pregnant With Second Child
S Club 7 To Reform?
S Club 7 Reuniting For Summer Tour (Test post)
Sweet Dreams My LA Ex
Rachel Stevens Robbed
Negotiate With Love
More, More, More


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