text:
\section{Introduction}
\label{sec:intro}
\begin{table*}
  \caption{Details of the sources/SWS spectra used in this study.}
  {\small
  \begin{tabular}{l@\  l l l l@\  l l@\  l}
    \hline
    \hline

    Source&
    IRAS name&
    AOT$^a$&
    TDT$^b$&
    Class.$^c$&
    SP98$^d$&
    Spec.Type$^e$&
    Remarks
    \\
    \hline
    \multicolumn{8}{c}{S stars from \citet{1994yCat.3168....0S} used in
    this study}\\
    \hline
    R And      & 00213+3817 & 01(2) & 40201723 & 2.SEc  & SE3 & S3,5-8,8e       & 18~$\mu$m feat. weak\\
    S Cas      & 01159+7220 & 01(2) & 41602133 & 3.SEp  & SE3 & S3,4-5,8e       & 15~$\mu$m feat., 18~$\mu$m feat. absent, C$_2$H$_2$+HCN abs.\\
    W Aql      & 19126-0708 & 01(2) & 16402335 & 3.SEp  & SE3 & S3,9-6,9e       & 15~$\mu$m feat., 18~$\mu$m feat. absent, C$_2$H$_2$+HCN abs.\\
    R Cyg      & 19354+5005 & 01(1) & 42201625 & 2.SEb  & SE3 & S2.5,9-6,9e     & 18~$\mu$m feat. absent, 10~$\mu$m feat. narrow\\
    $\chi$ Cyg & 19486+3247 & 01(2) & 15900437 & 2.SEb  & SE3 & S6,2-10,4e      & 18~$\mu$m feat. absent, substructure at 10.2~$\mu$m\\
    AA Cyg     & 20026+3640 & 01(2) & 36401817 & 2.M    & N   & S7,5-7.5,6      & :            \\
    RZ Sgr     & 20120-4433 & 01(2) & 14100818 & 2.SEa  & SE2 & S4,4ep          & \\
    $\pi^1$~Gru& 22196-4612 & 01(2) & 34402039 & 2.SEa  & SE2 & S7,5e           & 18~$\mu$m feat. absent \\
    RX Lac     & 22476+4047 & 01(1) & 78200427 & 2.SEa  & SE1 & M7.5Se          & :\\
    \hline
    \multicolumn{8}{c}{Stars from \citet{1994yCat.3168....0S} not included in the S star sample}\\
    \hline
    W Cet      & 23595-1457 & 01(2) & 37802225 & 2.SEa: & -   & S7$^{e1}$       & Low SNR\\
    T Cet      & 00192-2020 & 01(2) & 55502308 & 2.SEa  & SE1t& M5-6S IIe       & M supergiant, M, MS or S\\
    RW And     & 00445+3224 & 01(3) & 42301901 & 7      & SE3:& M5-10e(S6,2e)   & Low SNR\\
    WX Cam     & 03452+5301 & 01(2) & 81002721 & 1.NO   & -   & S5/5.5$^{e2}$   & Low SNR\\
    NO Aur     & 05374+3153 & 01(1) & 86603434 & 2.SEa  & SE1 & M2S Iab         & Supergiant\\
    LY Mus     & 13372-7136 & 01(2) & 13201304 & 1.NO   & -   & M4III$^{e1}$    & No dust features\\
    II Lup     & 15954-5114 & 06    & 29700401 & 3.CE$^{c1}$&-& SC$^{e3}$       & Carbon-rich\\
    ST Her     & 15492+4837 & 01(3) & 41901305 & 2.SEa  & SE1 & M6-7 IIIaS      & MS\\
    OP Her$^f$ & 17553+4521 & 01(1) & 77800625 & 1.NO   & N   & M5 IIb-IIIa(S)  & No dust features\\
    HD 165774  & 18058-3658 & 01(2) & 14100603 & 1.NO:  & -   & M2II/III$^{e1}$ & No dust features, low SNR\\
    S Lyr      & 19111+2555 & 01(1) & 52000546 & 2.CE:  & SE2 & SCe             & Low SNR\\
    HR Peg     & 22521+1640 & 01(2) & 37401910 & 1.NO   & -   & S5,1$^{e1}$     & No dust features\\
    GZ Peg     & 23070+0824 & 01(3) & 37600306 & 1.NO   & N:  & M4S III         & No dust features\\
    \hline
    \multicolumn{8}{c}{Supergiants with 10~$\mu$m features resembling the S stars}\\
    \hline
    KK Per     & 02068+5619 & 01(1) & 45701204 & 2.SEa  & -   & M2 Iab          & 18~$\mu$m feat. weak, UIR\\
    V605 Cas   & 02167+5926 & 01(2) & 61301202 & 2.SEa: & -   & M2 Iab$^{e4}$   & 18~$\mu$m feat. weak, UIR \\
    AD Per     & 02169+5645 & 01(2) & 78800921 & 2.SEap & -   & M2.5 Iab$^{e5}$ & 18~$\mu$m feat. weak, UIR\\
    NO Aur     & 05374+3153 & 01(1) & 86603434 & 2.SEa  & SE1 & M2S Iab         & 18~$\mu$m feat. weak, UIR \\
    V1749 Cyg  & 20193+3527 & 01(2) & 73000622 & 2.SEb  & SE3t& M3 Iab          & UIR\\
    IRC+40 427 & 20296+4028 & 01(3) & 53000406 & 2.SEap:& -   & M0-2 I$^{e6}$   & 18~$\mu$m feat. absent, UIR\\
    CIT 11     & 20377+3901 & 01(1) & 40503119 & 2.SEb  & -   & M3: Iab         & 18~$\mu$m feat. weak\\
    V354 Cep   & 22317+5838 & 01(2) & 41300101 & 2.SEc  & SE6 & M2.7 Iab        & 15~$\mu$m feat., 18~$\mu$m feat. absent\\
    V582 Cas   & 23278+6000 & 01(1) & 38501620 & 2.SEc  & SE5 & M4 I$^{e7}$     & 18~$\mu$m feat. weak, UIR:\\
    \hline
    \multicolumn{8}{c}{Other sources used in this study}\\
    \hline
    IRC+50 096 & 03229+4721 & 01(2) & 81002351 & 3.CE   & -   & C$^{e2}$        & Carbon-rich, ``30''~$\mu$m feature \\
    R Hya      & 13269-2301 & 01(1) & 08200502 & 2.SEa  & SE2t& M6-9eS(Tc)      & \\
    TY Dra     & 17361+5746 & 01(2) & 74102309 & 2.SEc  & SE8t& M5-8            & \\
    \hline
  \end{tabular}}\\
$^{a}$Observing mode used \citep[see][]{1996A&A...315L..49D,
  1996A&A...315L..38C}. Numbers in brackets correspond to the
scanning speed.
    $^{b}$TDT number which uniquely identifies each ISO observation.
    $^c$Classification of the SWS spectrum from
    \citet{2002ApJS..140..389K}, except
    $^{c1}$\citet{2003ApJS..147..379S}.
    $^d$IR classification in the scheme of
    \citet{1998ApJS..119..141S}.
    $^e$Spectral types are from \citet{1998ApJS..119..141S}, except
    $^{e1}$\citet{2001KFNT...17..409K},
    $^{e2}$\citet{2001yCat.3222....0B},
    $^{e3}$\citet{1998yCat.3206....0B},
    $^{e4}$\citet{1970AJ.....75..602H},
    $^{e5}$\citet{1955ApJ...122..434B},
    $^{e6}$\citet{1978A&AS...34..409S} and
    $^{e7}$\citet{1994AAS...185.4515W}.
    $^f$This source is only listed in the first edition of general
    catalogue of S stars \citep{1995yCat.3060....0S} and is classed M
    star in the second edition.
  \label{tab:smooth_sources}
\end{table*}
\begin{figure*}
  \sidecaption
  \centering \includegraphics[clip,width=12cm]{h12017f1}
  \caption{ISO/SWS spectra of the sources listed in
    Table~\ref{tab:smooth_sources}. From the bottom to the top we
    show. Eight spectra of S stars (S~Cas $-$ $\chi$~Cyg). The grey
    spectrum in the middle is R Hya, an O-rich AGB star that shows the
    typical structured 10~$\mu$m feature. Then nine M super-giants
    that exhibit a smooth and displaced 10~$\mu$m features (IRC+40~427
    $-$ V582~Cas). At the very top we show TY~Dra as an example of
    classical silicate dominated spectrum. The dashed lines represent
    the wavelengths of the substructures found in the O-rich AGB
    stars.}
  \label{fig:smoothies}
\end{figure*}
Asymptotic giant branch (AGB) stars are evolved stars of low to
intermediate mass in the ZAMS mass range of $\sim$1 to 8~M$_\odot$.
During the AGB phase, these stars are typified by high luminosity and
low surface temperature, which implies a very large radius and low
surface gravity. These stars often exhibit substantial mass loss
through a dust driven or pulsation driven wind. This mass loss is
important for several reasons. \emph{i)} These winds provide the means
through which these stars return nucleosynthesis products (i.e.
metals) from the interior of the star into the interstellar medium
(ISM). As the bulk of all stars fall in this mass range, the winds of
AGB stars are one of the dominant contributors to the enrichment of
the ISM. \emph{ii)} These dusty winds alter the appearance of these
stars because they cause the star to be surrounded by an envelope of
gas and dust. The dust will absorb the stellar radiation and reradiate
in the IR; therefore if one is to study the properties of these stars,
the dusty envelope needs to be taken into account. \emph{iii)} The
further evolution of the star is determined by the mass loss. Unlike
most types of stars, AGB star evolution is not determined by the
nuclear fusion processes in the interior but by the mass loss at the
surface and the AGB will end when the reservoir of envelope material
has been exhausted by the mass loss.

The type of molecules and solid-state particles that are present in
the winds are to the first order determined by the elemental
abundances at the surface of the star. Most important in this respect
is the number ratio of C-atoms to O-atoms (C/O ratio), because the
carbon-monoxide (CO) molecule is easily formed and very stable. This
causes most of the C- and O-atoms to be present in the form of CO.
These atoms are then effectively not taking part in the chemistry and
dust- condensation that occurs in these surroundings. Only the
fraction of either O-atoms if C/O is smaller than unity, or C-atoms if
C/O exceeds unity, is available. This dichotomy as a function of C/O
ratio is clearly found in the AGB stars. When C/O$<$1 , i.e. in O-rich
AGB stars, one finds large amounts of oxygen-bearing molecules, like
SiO, H$_2$O and CO$_2$, while for C/O$>$1, i.e. in C-rich AGB stars,
molecules like CH, C$_2$H$_2$ and HCN are present. The same holds for
the composition of the dust around these objects. The O-rich stars
exhibit silicates and oxides like amorphous aluminium-oxide
(Al$_2$O$_3$) or spinel, while their C-rich counterparts produce
amorphous carbon, silicon carbide and sulfides like MgS.

During the AGB phase the elemental abundances on the surface of the
star are being altered by a process called dredge-up. This causes
fusion products from the interior to be transported to the surface,
gradually increasing the C/O ratio. So, in the broadest possible terms
stars on the AGB gradually evolve from O-rich AGB stars to C-rich AGB
stars. In this scenario the S stars form an interesting intermediate
class of objects that have C/O$\simeq$1. Simplemindedly, one would
assume that in such surroundings the range of molecules and dust
components could be very wide perhaps overlapping with both the
typical O-rich and C-rich species or species that are not found in
either surroundings. Theoretically, iron-silicide and metallic iron
are the dust species predicted on the basis on chemical equilibrium
calculations \citep{2002A&A...382..256F}. Observationally, this class
of objects has not been exhaustively studied to determine the dust
composition although some studies have focused on the 10~$\mu$m
emission feature from S stars \citep{1988ApJ...333..305L,
  1993ApJ...416..769C, 1998ApJS..119..141S, 2000A&AS..146..437S}. In
particular the spectra obtained with the Short Wavelength Spectrometer
(SWS) \citep{1996A&A...315L..49D} on-board the Infrared Space
Observatory (ISO) \citep{1996A&A...315L..27K} which cover a much
broader wavelength range (2$-$45~$\mu$m) than available before with a
high sensitivity and spectral resolving power, allow us to get a more
complete picture of the composition around S stars.

The most diagnostic feature in the S star spectra is found in the
10~$\mu$m region. The dust emission features in the 10~$\mu$m region
are very extensively studied because \emph{i}) this window is
available for ground-based observations, \emph{ii}) it holds the
important diagnostic resonances of both O-rich (silicates, Al$_2$O$_3$
and spinel) and C-rich (SiC) dust and \emph{iii}) spectra for many
evolved stars in this region are available in the form of IRAS/LRS
spectra. Many studies have focused on classifying the spectral
appearance of the $\sim$10~$\mu$m emission band, using various
classification schemes, and relating the classification to the other
observable characteristic of the sources like the spectral type,
luminosity class, the C/O ratio, the variability type or the mass-loss
rate \citep{1988ApJ...333..305L,1990MNRAS.243...78S,
  1990AJ.....99.1173L,1993ApJ...416..769C,1995ApJ...451..758S,
  1998ApJS..119..141S,1999MNRAS.309..180S,2000A&AS..146..437S,
  2000ApJ...531..917M,2002ApJS..140..389K,2007A&A...463..663Y}. Here
we do not repeat the details of these studies but focus on the main
conclusions that are relevant for the current work and refer to
\citet{1998ApJS..119..141S} and \citet{2000A&AS..146..437S} for
extensive and thorough comparisons of the relevant literature and the
various interpretations of the dust emission characteristics.

The main points that have emerged are as follows:
\begin{enumerate}
\item O-rich AGB stars show a range of dust emission features with a
  range of peak positions.
  \begin{enumerate}
  \item A single narrow peak at 9.7~$\mu$m (on a F$_\nu$ scale), due to
    ``classical silicates''. The corresponding Si-O bending mode
    resonance is also observed near 18~$\mu$m.
  \item A broader structured feature, with local maxima at 9.7, 11 and
    13~$\mu$m, with the peak-position close to $\sim$10~$\mu$m.
  \item A broad and shifted feature peaking at longer wavelength (up
    to 13~$\mu$m). This broad feature exhibits the same local maxima
    as mentioned above. It is generally accepted that this broad
    feature is due to the dominant contribution of dust components
    other than the silicates, probably amorphous aluminium-oxide
    \citep{1989A&A...218..169O}.
  \end{enumerate}
  The origin of the structured features (b) in between the two
  extremes above is uncertain. While \citet{1989A&A...218..169O}and
  \citet{2000MNRAS.315..856L} model these spectra with a mixture of
  silicates and aluminium-oxide, \citet{2001ApJ...558..165E} find that
  these observations, with the additional constraints set by the IRAS
  broadband photometry, are best explained using pure silicates in a
  dust shell of larger optical depth. However, the fact that one finds
  the same substructures within a wide range of peak-positions argues
  against the opacity effect being dominant, and most likely these
  sources represent a mixture of silicate and aluminium-oxide grains.
\item M super-giants exhibit a similar range of 10~$\mu$m features,
  although they are more weighted to the classical silicate profiles
  (a) and the broad (c)-type features are rare
  \citep{1998ApJS..119..141S}. An interesting exception is a
  significant fraction of M super-giants of the h and $\chi$~Per
  association that exhibit a (c)-type feature peaking near 10.5~$\mu$m
  with the 11.3~$\mu$m UIR band perched on top
  \citep{1998MNRAS.301.1083S}. In Sect.~\ref{sec:discussion} we will
  compare these interesting sources with the S stars.
\item \citet{1988ApJ...333..305L} find that S-type stars
  preferentially exhibit a broad feature peaking in the
  10.5$-$10.8~$\mu$m range, which in fact makes them dub this feature
  the ``S'' feature. This agrees well with the findings of
  \citet{1998ApJS..119..141S}, who also find that the S-type stars in
  their sample predominantly exhibit such a broad feature. In contrast
  \citet{1993ApJ...416..769C} report that the S-type stars have
  emission features very similar to M stars, covering the complete
  range from pure silicates to the broad feature profile. This
  difference is easily understood from the fact that the latter
  authors include in their much larger sample also many MS and weak S
  stars which have a C/O ratio well below unity and should have dust
  similar to the M stars. The profile found in the strong S stars is
  broad and peaking in the 10.5$-$10.8~$\mu$m range. The extend and
  peak-position of this S star feature are very similar to the broad
  features found in the O-rich AGB stars, however the 13~$\mu$m
  feature is lacking in the S star spectra
  \citep[][Fig.9]{1998ApJS..119..141S}. These authors also find that
  there might be a slight enhancement between 10 to 11~$\mu$m in the
  S-type feature when compared to the M star sample, although they
  state that the difference might not be significant given the quality
  of the LRS spectra they used.
\end{enumerate}

In this paper we explore the dust composition around S stars as
derived from the available SWS spectra.

\section{Observations}
\label{sec:observations}
The ISO/SWS database contains 22 S star spectra that cover the full
wavelength range of 2.3-45~$\mu$m: 21 ISO/SWS sources listed in the
second edition of the general catalogue of S stars
\citep{1994yCat.3168....0S} with the addition of the S star OP~Her are
given in Table~\ref{tab:smooth_sources}. Of these 22 sources we
include nine in the S star sample that we explore here; NO~Aur is a
super-giant, II~Lup is carbon-rich, ST~Her is an MS star and T~Cet is
of uncertain nature. The other stars have either no significant dust
emission or too little signal-to-noise to investigate their dust
composition to the level of detail required here.

\subsection{Data reduction}
The data were processed using SWS interactive analysis, IA
\citep[see][]{1996A&A...315L..49D}, using calibration files and
procedures equivalent to pipeline version 10.1. Further data
processing consisted of extensive bad data removal and rebinning on a
fixed resolution ($\lambda$/$\Delta\lambda$=200) wavelength grid. In
order to combine the different sub-bands into one continuous spectrum
from 2 to 45 $\mu$m we applied scaling factors. In general the match
between the different sub-bands is good and the applied
scaling/offsets are small compared to the flux calibration
uncertainties with a few exceptions:

\subsubsection{$\chi$ Cyg }
The band 2A (4.1$-$5.3~$\mu$m) and 2C (7.0$-$12.5~$\mu$m) data are
affected by strong memory effects. The shapes of band 2A of the up and
down scans differ substantially. The slope of the band 2C data differs
while the details of the shape and substructure are present in both
scans. The data appear to be also slightly affected by miss-pointing
as we have to apply a scaling of $\sim$1.08 to the band 1
(2.4$-$4.1~$\mu$m) data and 1.2 to the band 3 (12.5$-$29~$\mu$m) data.

\subsubsection{$\pi^1$~Gru}
The data for $\pi^1$~Gru are apparently affected by a slight
miss-pointing and the data for the sub-bands 2A to 3D (4.1 $-$ 27.5
$\mu$m) need to be multiplied by a relatively large factor
($\sim$1.25) to be consistent with the flux levels at shorter and
longer wavelengths. We note that the main signature of the MgS feature
is contained within sub-band 3D (19.5 $-$ 27~$\mu$m) and is not
affected by the scaling (see also Fig.~\ref{fig:updown}).

The final reduced spectra are presented in Fig.~\ref{fig:smoothies}.
As it turns out these stars are very rich in their dust emission
spectra exhibiting a wide range of dust features from different types
of materials. We will first discuss the long wavelength part of the
spectra of \object{$\pi^1$ Gru}, \object{W Aql} and \object{RX Lac} as
they show features that have not been detected before around S stars.

\section{Long wavelength spectra}
\begin{figure}
  \centering \includegraphics[clip,width=8.8cm]{h12017f2}
  \caption{Comparison of the features found in the SWS spectra of
    $\pi^1$~Gru and W~Aql to the MgS feature in IRC+50~096. We show
    the signal of the two independent scans of sub-band 3D. The
    characteristic sharp rise from 24 to 26 (indicated in the light
    shaded area) with a gradual decline towards longer wavelength is
    found in all available scans. The scale along the ordinate is
    chosen to better bring out the structure in this wavelength domain
    without having to resort to removing an underlying baseline. The
    dotted line shows the spectral signature expected from a star
    surrounded by MgS, simulated with a Planck-function of 1200~K plus
    the emission of MgS grains at 500~K in a CDE-shape distribution.
    Near the bottom we show the spectrum of the MS star ST~Her as an
    example of a source that does not show this feature.}
  \label{fig:updown}
\end{figure}
\begin{figure}
  \centering
  \includegraphics[width=8.8cm]{h12017f3}
  \caption{Long wavelength spectra of RX~Lac and AA~Cyg. The intensity
    units are chosen to better exhibit the emission bands on the
    steeply dropping stellar continuum. Below we show the absorption
    cross-sections of Diopside
    \citep[MgCaSi$_2$O$_6$,][]{2000A&A...363.1115K}}
  \label{fig:rx_lac}
\end{figure}

\subsection{The ``30 $\mu$m'' feature}
In Fig.~\ref{fig:spec_overview} we show the spectra of $\pi^1$~Gru and
W~Aql.  We also show for comparison the SWS spectrum of the C-rich red
giant \object{IRC+50~096}, which exhibits purely C-rich dust features
and the MS star \object{ST~Her}, which exhibits O-rich dust features.

The most remarkable feature in the spectra of these two S stars is the
emission feature starting at 23.5~$\mu$m and peaking at 26~$\mu$m,
indicated in Fig.~\ref{fig:spec_overview} with MgS. The feature is
weak and even in the closeup of the region in the right panel of
Fig.~\ref{fig:spec_details} not very prominent. This is probably also
the reason why it has eluded detection until now.

In Fig.~\ref{fig:updown} we display the spectra in intensity units
that better reveal the structure in this region. The shape of the
feature found in the S star spectra closely corresponds to the shape
of the much stronger MgS resonance found in the C-rich star
IRC+50~096. In particular the change of slope from 22 to 24 $\mu$m and
the second change beyond 26 $\mu$m is detected in the three sources at
the top. We also show the expected spectrum from MgS, which exhibits
the same shape. The two independent scans in the SWS data yield the
same shape, attesting to the reality of the MgS detection.

The presence of MgS around these stars is unexpected and prompts
several questions on dust condensation conditions around such stars.
It is important to also take into account other aspects of these
systems. First we will discuss the other dust features in the spectra
of these stars and subsequently the molecular composition.

\subsection{RX Lac and AA Cyg}
In Fig.~\ref{fig:rx_lac} we show the spectra of RX~Lac and AA~Cyg.
Both sources exhibit structure at 20, 32.5 and 40~$\mu$m. The
structure around 20~$\mu$m seems to be quite secure in both spectra.
The long wavelength part of the AA~Cyg spectrum is very noisy.
Comparing the detected features with available laboratory spectra they
seem to correspond best to Diopside. There might be a connection
between the appearance near 10~$\mu$m as both sources exhibit a weak,
very red emission feature and strong SiO absorption. This absorption,
in combination with a low Diopside temperature, might explain why we
do not detect the corresponding 10~$\mu$m bands of Diopside. In should
be borne in mind that the long wavelength spectra of these stars are
quite noisy and that the correspondence with the laboratory spectrum
is not perfect. In particular the 25~$\mu$m feature which is present
in the laboratory spectrum is markedly absent in the stellar
emissions. Therefore this should be considered a tentative
identification.

\section{The broad feature in the SWS spectra of S stars}
\begin{figure}
  \centering \includegraphics[clip,width=8.8cm]{h12017f4}
  \caption{Overview of the SWS spectra of four red giant stars. We
    show from top to bottom the carbon-rich AGB star IRC+50~096, the
    M6.5S star ST~Her and the S stars $\pi^1$~Gru and W~Aql. The
    carbon-rich star exhibits the typical SiC feature at 11.3 $\mu$m
    and the MgS feature near 26 $\mu$m. The ST~Her spectrum is
    dominated by the silicate dust features at 10 and 20 $\mu$m which
    are typical for oxygen-rich environments. $\pi^1$~Gru and W~Aql
    exhibit the MgS feature (see also Fig.~\ref{fig:spec_details} \&
    \ref{fig:updown}) and a broad feature around 10 $\mu$m which
    resembles the silicate emission but is lacking clear evidence of
    the corresponding 20~$\mu$m silicate band. The latter is
    especially clear in the spectrum of $\pi^1$~Gru, while there is a
    weak feature near $\sim$17~$\mu$m in the spectrum of W~Aql.}
  \label{fig:spec_overview}
\end{figure}
\begin{figure*}
  \centering \includegraphics[clip,height=18cm,angle=90]{h12017f5}
  \caption{Detailed view of the IR spectra of the stars presented in
    Fig.~\ref{fig:spec_overview}. The left panel shows the shortest
    wavelength region in which the spectral structure is dominated by
    molecular absorption bands. Clearly the molecular composition of
    $\pi^1$~Gru resembles that of ST~Her. The typical C-rich molecular
    bands due to C$_2$H$_2$, HCN and C$_3$ are absent in $\pi^1$~Gru
    but are seen in the IRC+50~096 and W~Aql. The middle panel
    compares the 10 to 20 $\mu$m range of these sources. The
    wavelength range of the broad $\sim$10~$\mu$m emission band in the
    S star spectra is identical to the silicate emission of ST~Her,
    however the feature appears more smooth and the sharp
    substructures at 9.5, 10.8 and 13 $\mu$m are absent. Likewise, the
    20~$\mu$m silicate band is not observed. The silicon-carbide feature
    seen in IRC+50~096 corresponds in peak position but is much
    narrower than the emission feature in ST~Her. Finally, the panel
    on the right shows the MgS emission feature which is detected in
    the IR spectra of $\pi^1$~Gru, W~Aql and IRC+50~096 and not in
    ST~Her.}
  \label{fig:spec_details}
\end{figure*}
\begin{figure}
  \includegraphics[width=8.8cm]{h12017f6}
  \caption{Comparison of the mean profiles of the S stars and the
    O-rich stars. The samples have been split in two parts. Those with
    profiles peaking beyond 10.5~$\mu$m (top panel) and those that
    peak at shorter wavelengths (bottom panel). The dashed line
    indicates the position (10.3~$\mu$m) where the mean profiles
    differ significantly. For reference we also show the feature
    spectrum of TY~Dra, which shows a classical silicate emission
    feature. The spectrum has been offset for clarity.}
  \label{fig:mean_profiles}
\end{figure}
\begin{figure}
  \includegraphics[width=8.8cm]{h12017f7}
  \caption{Properties of the M and S stars. From top to bottom: the
    fitted temperature of the (reddened) stars; the ratio of the
    excess to the stellar flux and the ratio of the flux in the
    feature to the flux in the dust excess. The S stars in the sample
    are clearly cooler (i.e. more extincted) and show more excess
    than the M stars.}
  \label{fig:measurements}
\end{figure}
The most prominent dust feature in the spectra of these S stars is the
broad and smooth emission feature centred around $\sim$11~$\mu$m
(Fig.~\ref{fig:spec_overview} and the middle panel of
Fig.~\ref{fig:spec_details}). A similar feature (covering the same
wavelength range) is found in the IR spectra of many O-rich evolved
stars
\citep[e.g.][]{1968ApJ...154..677G,1990AJ.....99.1173L,2002ApJS..140..389K},
which it is usually attributed to a combination of silicates and
aluminium-oxide with the possible addition of spinel at 13~$\mu$m
\citep[e.g.][]{1969ApJ...155L.181W,1972A&A....21..239H,1999A&A...352..609P,Cami_PhD}.
However, the corresponding silicate feature due to the Si-O
stretch/bend near 18~$\mu$m is remarkably weak.

The similarities between the S star 10~$\mu$m features and the broad
feature found in the O-rich spectra have until now been interpreted as
the S stars showing silicate plus aluminium-oxide emission like the
O-rich stars. In the following we will argue against this
interpretation. Instead, we will show that there is a significant
difference between the M star broad features due to silicates plus
aluminium-oxide and the S star broad features, pointing to a different
dust composition for these S stars. In the following we concentrate on
comparing the S star spectra with O-rich stars that exhibit low dust
columns, since these O-rich stars show the structured 10~$\mu$m
emission complex. The stars that have higher mass-loss rates show
profiles close to the classical silicate emission
\citep[e.g.][]{2005A&A...439..171H}. See TY~Dra in
Fig.~\ref{fig:smoothies} for an example of such a classical silicate
feature.

We readdress the issue of the spectral appearance of the 8$-$22~$\mu$m
dust spectra of the S stars using the available SWS spectra. We choose
to restrict ourselves to the relatively small sample of SWS spectra
for several reasons. The first reason is to have a consistent data
set. More importantly, the sensitivity and spectral resolving power
allow us to discuss details not available in the LRS spectra or in
many of the ground-based spectra. As an example we mention \object{R
  Aql} for which \citet{2000A&AS..146..437S} report a broad feature
without detectable substructure based on their CGS3 spectra, while the
SWS spectra clearly resolve the substructures at 9.7, 11 and
13~$\mu$m. Finally, the much wider wavelength coverage allows us to
better separate the different molecular and dust contributions. For
example, the 10~$\mu$m region feature of the Mira variable \object{RR
  Per} resembles the S star spectra. However, the complete SWS
spectrum reveals very strong molecular absorption and emission bands.
This spectrum could have been misinterpreted, in case only the 8 $-$
22~$\mu$m range would had been available.

\citet{2002ApJS..140..389K} have classified the ISO/SWS spectra
according to the shape of the continuum and dust features. Within
their classification $\pi^1$~Gru, W~Aql and many O-rich stars belong
to the same class exhibiting the broad feature due to silicate and
aluminium-oxide. Although the peak position and wavelength extend of
the emission bump are indeed very similar, the O-rich sources show
more substructure with often a prominent sharp emission maximum at
13~$\mu$m and always substructure at 9.7 and $\sim$11~$\mu$m
\citep[e.g.][ see also Fig.~\ref{fig:spec_details}]{Cami_PhD}. This
substructure is not found in the spectra of $\pi^1$~Gru and W~Aql.

A careful survey of all evolved star spectra with sufficient signal to
noise in the SWS database yields 9 more sources with a broadened and
smooth $\sim$10~$\mu$m emission feature. These sources are listed in
Table~\ref{tab:smooth_sources} and their spectra are shown in
Fig.~\ref{fig:smoothies}. The main conclusion we draw is that such a
broad and smooth emission feature is only found in the M super-giant
and the S star spectra, \emph{there are no O-rich AGB stars that
  exhibit the same emission feature}. This agrees very well with the
findings of \citet{2000A&AS..146..437S} that the broad feature in the
AGB stars differs from the broad features found in the super-giants.
The ISO spectra show that in fact the broad O-rich AGB star features
are always due to a mixture of the 9.7, 11 and 13~$\mu$m bands in
which the 11~$\mu$m band dominates. Admittedly the substructures are
sometimes more pronounced than in other cases which leaves open the
possibility that part of the emission in this region, even in the
O-rich AGB stars spectra, is due to the same smooth feature present in
the S stars. $\chi$~Cyg is the only S star that has exhibits these
substructures although the predominant contribution might still be a
smooth underlying feature.

Note that the sample of M super-giants displayed in
Fig.~\ref{fig:smoothies} largely overlaps with the broad featured M
super-giants presented by \citet{2000A&AS..146..437S} and consists
mostly of super-giants located in the h and $\chi$~Per association.
These sources are by no means typical for all galactic M super-giants.
As we already pointed out, the large majority of studied M
super-giants exhibits a classical silicate emission feature
\citep{1998ApJS..119..141S,2000A&AS..146..437S}. Moreover, seven out
of the nine broad featured M super-giants in our sample reveal UIR
emission bands, which are not commonly found in the M super-giant
spectra \citep{1994MNRAS.266..640S,1998MNRAS.301.1083S}.
\citet{1998MNRAS.301.1083S} suggest that this could be related to
peculiar elemental abundances at the stellar surfaces.

Another striking aspect of these spectra as a group is the relative
strength of the 10~$\mu$m feature compared to the 18~$\mu$m feature.
In the spectra of the O-rich stars, the 10~$\mu$m emission is
accompanied by an emission feature near 18$-$20~$\mu$m, where one
would expect the Si-O bending modes of the silicates to be present
(see Fig.~\ref{fig:spec_details}). This emission band is
systematically weak in the M super-giant and S star spectra in
Fig.~\ref{fig:smoothies}. In some of the sources we find no evidence
of the 18~$\mu$m band at all and three sources exhibit a weak emission
band near 15~$\mu$m instead.

\subsection{Feature extraction}
The differences in the observed features as discussed above are
relatively subtle. In order to enhance the contrast we have removed
the ``continuum'' from the spectra. We stress that the continuum as
such does not have any clear physical meaning in this context as the
same material(s) that give rise to the features contribute to this
continuum. It represents only a means to remove those contributions
that do not give rise to spectral signatures. It further allows us to
compare the relative strength of the remaining bands to other
components. Because of the wide range of properties of the stars in
the sample -- in terms of optical depth, strength of the molecular
bands and the excess -- we have opted to use a crude method for
continuum estimation. The continuum is represented by a sum of a warm
black-body-function (F$_\nu$ = B$_\nu$(T); the reddened stellar
photosphere) and a cooler modified black-body-function (F$_\nu$ =
$\nu^{p}~\times~$B$_\nu$(T); the dust excess). These two functions are
fitted simultaneously to selected ``continuum-points''. The latter are
difficult to define unambiguously and we choose to use the following
ranges: 2.9$-$3.35~$\mu$m, when the molecular absorption is not too
prominent; 3.35$-$3.8~$\mu$m; 7$-$7.5$^\dagger$~$\mu$m;
8.5$-$9.5$^\dagger$~$\mu$m; 14$-$15~$\mu$m; 22$-$25~$\mu$m and
36$-$44~$\mu$m. The ranges marked with a dagger often do not exhibit
clear continuum character. These regions have still been included,
albeit with a reduced weight, to account for the fact that the
continuum should run close to them.

The resulting residual spectra have been co-added to reduce the noise.
The co-addition has been applied in two bins, depending on the
peak-position of the ``10''~$\mu$m emission feature. The results are
shown in Fig.~\ref{fig:mean_profiles}, where we compare the S star
profiles to the features found in O-rich stars. Note that the
comparison is done on the basis of the extracted feature and does not
follow strictly the silicate-index classification. We find that both
S-star SEa and SEb classes compare best with the O-rich SEa class and
the S-star SEc class with the O-rich SEb class. This mismatch reflects
the fact that the underlying continua differs systematically -- the
O-rich stars being bluer -- between both groups of sources (see also
below).

Fig.~\ref{fig:mean_profiles} demonstrates that indeed the O-rich star
exhibit a ``10''~$\mu$m feature which is composed of three distinct
components while the S star spectra exhibit only a single broad
emission band -- indicative of a different dust composition between
the two groups. There are several other ``properties'' of these dust
spectra that change in league with the differences in dust
composition. The lack of the 19.5~$\mu$m band in the S star spectra is
pronounced. In Fig.~\ref{fig:measurements} we summarise the derived
properties of the S stars compared to those of the M stars. The main
conclusion is that the studied S stars as a sample are redder and
exhibit a stronger excess than the O-rich stars with the broad
10~$\mu$m feature. This indicates the presence of more dust along the
line of sight towards the S stars. There is no significant difference
in the strength of the 10~$\mu$m feature relative to the dust
continuum (Fig.~\ref{fig:measurements}c).

\section{Discussion}
\label{sec:discussion}
As discussed above, the spectral appearance of S stars is
significantly different from the O-rich AGB stars. Here we explore the
possible explanations for these differences, that is, the relative
strength of the emission bands and the displacement of the 10~$\mu$m
feature. The amount of mid-IR excess is probably not directly related
to the dust composition. Perhaps the observed difference in dust
composition and the differences in the quantities of dust share a
common origin in the particular condition that prevail during the S
star evolutionary state.

There are several effects that, if at work, will influence the
spectral appearance of dust features even arising from grains with the
same chemical composition. The most notable are dust temperature and
grain-size. Using the amorphous olivine
(Mg$_{0.8}$Fe$_{1.2}$SiO$_{4}$) that explains (part of) the emission
of the O-rich stars well \citep{2005A&A...439..171H}), we find that
the temperature required to explain the observed S star
10-to-18~$\mu$m ratio (ignoring the mismatch in peak-position) needs
to be higher than 2000~K. And even at such high temperatures (well
above the evaporation temperature of silicates) the feature at
18~$\mu$m would still be too prominent for the most extreme cases,
e.g. \object{$\pi^1$ Gru} or \object{W Aql}. Thus, dust temperature is
excluded as the cause of the weak 18-20~$\mu$m features.

Grain-size: We have simulated the effects of grain-size on the
spectral features of silicates based on simulated optical properties
using a Mie calculation \citep{BohrenHuffman}. The effect of
increasing the grain-size from 0.01 to 1 $\mu$m is indeed a
displacement of the 10~$\mu$m emission feature, but the effect is
subtle and it moves the peak by less than 0.3~$\mu$m. This is not
enough to explain the S star spectra. Moreover the ratio of the 10 to
18~$\mu$m band is only slightly affected. The 18~$\mu$m band does not
shift significantly but becomes somewhat stronger. The S star
spectra exhibit an 18~$\mu$m feature which is little pronounced and
peaks at shorter wavelength. We conclude that the grain-size is not
the dominant factor for explaining the S star silicate feature.

The paper by \citet{2003A&A...408..193J} is very interesting in terms
of the compositional influence on the silicate emission. These authors
have studied the IR transmission spectra of non-stoichiometric
magnesium-rich silicates. They find that there is a significant shift
of the 10~$\mu$m Si-O stretching resonance as a function of the Mg to
SiO$_4$ ratio. The trend is such that as the Mg to SiO$_4$ ratio
increases, the 10~$\mu$m peak shifts to longer wavelength, the
18~$\mu$m band broadens and weakens compared to the continuum and
shifts to shorter wavelength. This mimics to a large extent the
behaviour observed in the S star spectra. It should be noted that
although the 10~$\mu$m feature in the laboratory spectra shifts by a
large amount ($>$1~$\mu$m), it is not completely sufficient to explain
the full range observed in the stellar spectra. If the observed shift
is indeed linked to the presence of non-stoichiometric silicates, than
there could be an obvious connection to the photospheric abundances
since the Mg to SiO$_4$ ratio in the silicate might measure the Mg to
free O or SiO in the gas phase. In case of C/O $\sim$ 1 there is more
Mg in relative terms and those non-stoichiometric silicates may form.

Moreover, the M-super-giants that we present are special not just in
their 10~$\mu$m spectrum but also because they exhibit a dual
chemistry with both silicates and PAHs. How this dual chemistry comes
about is at present unclear. This may be evidence of the presence of a
disk plus wind geometry, shocked regions in the outflow or an
abundance pattern in the outflow, which permit this dual chemistry to
exist. In any case, it is clear that in some region of the
circumstellar environment the chemistry should be close to a C/O
around unity.

It should be stressed that we cannot draw general conclusions about
the dust formation around S stars from such a small number of sources.
We have successfully proposed to observe 90 S stars with IRS
\cite{2004AAS...204.3304H} on Spitzer (GO-30737, PI. Hony). The main
findings of the current paper, i.e., the presence of the MgS feature
and the shifted 10~$\mu$m feature, are borne out by the spectra
obtained in the Spitzer sample (Smolders et al, in prep). Because of
the larger sample the range of spectral features, in particular in the
10-20~$\mu$m region is larger than what is presented here.

\section{Conclusions}
We have presented a detailed study of dust spectra of the S stars
observed by ISO/SWS. The spectra exhibit several unique dust
characteristics. In particular, we find two S stars ($\pi^1$~Gru and
W~Aql) that exhibit a weak ``30''~$\mu$m feature due to MgS grains. RX
Lac and \object{AA Cyg} exhibit features between 20$-$40~$\mu$m which
may be related to Diopside, although this is at most a tentative
identification. The 10~$\mu$m region of the dust-producing S stars
stands out due to its smooth and broad emission feature. The feature
is located clearly at longer wavelengths than the classical silicate
feature, without showing the characteristic substructure found in the
spectra of the O-rich AGB stars with a broad 10~$\mu$m feature. The
peculiar 10~$\mu$m features of the S stars are accompanied by very
weak or absent features near 18~$\mu$m. We conclude that S stars make
different types of dust than the O-rich AGB stars, including those
that exhibit shifted 10~$\mu$m features. As a group the S stars and
their dust shells do not compare well to the O-rich AGB stars with
structured features, the S stars are redder and produce more dust. The
common explanation for the shifted 10~$\mu$m band, i.e. a mixture of
classical silicate with aluminium-oxide, does not appear to apply to
the S stars. We have explored possible origins of the peculiar
spectra. We find that non-stoichiometric silicates with an increased
Mg to SiO$_4$ ratio might be at the origin of the displaced emission.
Interestingly, the properties of the peculiar 10 and 20~$\mu$m
features are shared with a small subgroup of M super-giants. These
super-giants, which are preferentially found in the h and $\chi$ Per
associations, also exhibit the UIR emission features, again
strengthening the possible link with the abundances in the dust
forming regions.

\begin{acknowledgements}
  IA$^3$ is a joint development of the SWS consortium. Contributing
  institutes are SRON, MPE, KUL and the ESA Astrophysics Division.
  This work was supported by the Dutch ISO Data Analysis
  Center(DIDAC). The DIDAC is sponsored by SRON, ECAB, ASTRON and the
  universities of Amsterdam, Groningen, Leiden and Leuven.
\end{acknowledgements}

\bibliographystyle{aa}


text:
National Cowboy and Western Heritage Museum
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The National Cowboy & Western Heritage Museum is America's premier institution of Western history, art, and culture. Founded in 1955, the Museum, located in Oklahoma City, collects, preserves, and exhibits an internationally renowned collection of Western art and artifacts while sponsoring dynamic educational programs to stimulate interest in the enduring legacy of the American West. More than 10 million visitors from around the world have sought out this unique museum to gain better understanding of the West: a region and a history that permeates our national culture.
The National Cowboy & Western Heritage Museum features a superb collection of classic and contemporary Western art, including works by Frederic Remington and Charles M. Russell, as well as sculptor James Earle Fraser's magnificent work, The End of the Trail. The exhibition wing houses a turn-of-the-century town and interactive history galleries that focus on the American cowboy, rodeos, Native American culture, Victorian firearms, frontier military, and Western performers. Outside, beautifully landscaped gardens flank the Children's Cowboy Corral and interactive children's space.
From fine art, pop culture, and firearms to Native American objects, historical cowboy gear, shopping, and dining, the Museum tells America's story as it unfolds across the West.
MISSION STATEMENT The National Cowboy & Western Heritage Museum preserves and interprets the evolving history and cultures of the American West for the education and enrichment of its diverse audiences of adults and children.
E-mail: marketing@nationalcowboymuseum.org
Website: nationalcowboymuseum.org
1700 NE 63rd St
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National Cowboy and Western Heritage Museum schedule:
2016-08-26 01:00:00 (Ended) Power & Prestige: Headdresses of the American Plains Find Tickets
2016-10-14 01:00:00 (Ended) Cowboy Artists of America 51st Annual Sale & Exhibition Find Tickets
2016-10-14 01:00:00 (Ended) Traditional Cowboy Arts Association 18th Annual Exhibition & Sale (TCAA) Find Tickets
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German (Lubeck) 19th century. Stolle was a painter of Portraits and architectual views who studied with his father, the Lubeck painter and decorative artist Johann Wilhelm Stolle. Most of his paintings are still owned by his family although there are several drawings and watercolours by him which can be seen at the Museum in Lubeck.


CA24 (Santa Barbara): Apologies to my wonderful subscribers, as I was waiting for confirmation about Lois Capps retirement plans and missed the early distribution. Anyway, it looks as if it's Helene Schneider (D-Santa Barbara) Laura Capps (D-Santa Barbara), Katcho Achadjian (R-Arroyo Grande) and Justin Fareed (R-Santa Barbara) running to succeed the 17-year congresswoman. Other possible candidates include Salud Carbahal (D-Santa Barbara) supervisor and Chris Mitchum (R-Santa Barbara). Assemblymember Das Williams will likely make a decision based on what Carbahal does, as the termed-out Assemblymember is in a holding pattern pending a vacancy in Hannah Beth Jackson's State Senate seat.
JOB HUNTING: Meanwhile, Senate Minority Leader Bob Huff is announcing today that he'll run to succeed Mike Antonovich next year for the LA County Board of Supervisors.
MONEY MATTERS: As the May revision approaches, California Forward has a new report on financing California's future.
JACKALOPE: Extending Prop 30 by Camouflage [Joel Fox] - "Those who would support such an effort would probably have us believe we are not looking at a jackrabbit but we see a jackalope–a mythical figure that belongs in the same league as a another seemingly mythical figure– a temporary tax."
#CAKEDAY: Happy birthday to Gregory "Flap" Cole, Nicole Fossier, and Andy Katz!
Join Capitol Network for its Spring Luncheon featuring Debbie Manning, the first female California State Senate Chief Sergeant-at-Arms. April 23 at 11:30am at Cal Chamber 1215 K Street, Suite 1400, California Room. Click here to register: capitolnetwork.wildapricot.org/event-1848721. For more info, email alevy@cpapsych.org.
Corporate & Individual Sponsorships - Available for 8th Annual Assembly Veterans of the Year Luncheon, Wednesday, June 24th. Event co-sponsored by major veterans groups. Last year 75 Assemblymembers honored district veterans, 350 people attended.
Planned Parenthood Affiliates of California seeks experienced lobbyist to work on policy issues related to reproductive health, health care, ACA, Medi-Cal and women's health. Competitive salary and excellent benefits package. Details here.
Join Emerge California's 3rd Annual Sacramento Reception on Tuesday, April 14 from 6:30pm to 8:30pm at the Metropolitan Terrace – Citizen Hotel located at 926 J. St in Downtown Sacramento. To join the Host Committee, please contact Nazneen Rydhan-Foster at naz@emergeca.org or visit the event page here.
California Nurses Association seeks Regulatory / Policy Specialist to help improve healthcare for California patients. Do you have firsthand Sacramento experience helping to develop laws, policies, or regulations? Permanent full time position. Excellent benefits - family healthcare, pension, 401k. If needed, will help the right person making a long term commitment learn more about health care, and nursing regulations.
Democratic Congressman seeks highly-motivated individual to serve as Member's DC Scheduler, who will evaluate and respond to meeting requests among other duties. The office's atmosphere is supportive with opportunities for professional growth. Spanish-speaking candidates preferred. Please send resume to californiascheduler@mail.house.gov.
Learn the legislative process and best practices for effective lobbying. Cover the complete spectrum of governmental advocacy in two days, including the legislature, budget advocacy, regulatory agencies, the administration, and media relations. Capitol veteran Ray LeBov presents "Lobbying 101" and "Lobbying 201" seminars April 23-24. $250 each. Essential for lobbying firm principals / support staff, organizations / public agencies that employ lobbyists. Complete info / registration: www.capitolseminars.net or 916 442 5009.
Add your 100-word classified for $30/week. Email me at scott@scottlay.com.
An advocacy group has filed a lawsuit seeking to stop teachers unions in California from using member dues for political purposes unless individual instructors provide their permission.
But the Legislature has plans of its own, and a proposal sponsored by the state Senate's top Democrat won unanimous approval Wednesday from the Senate Higher Education Committee.
Latino lawmakers, who have increasingly flexed their muscle as a voting bloc in the Capitol, released their list of priority bills Wednesday, including efforts to increase voter registration and promote clean energy.
Actuaries recommend a $487.2 million annual increase in state payments to CalPERS in the new fiscal year that begins in July, an increase for state worker pensions of about 10 percent to $4.9 billion.
Frustration with development continues to loom large in a race to represent a Los Angeles council district that stretches from Sherman Oaks to the Miracle Mile, as one candidate pledged to swear off campaign money from developers and another pointed out her rival recently sold property to a developer.
Latino lawmakers, who have increasingly flexed their muscle as a voting bloc in the Capitol, endorsed a slate of proposals Wednesday that includes efforts to increase voter registration and promote clean energy.
Protesters in San Diego took to the streets Wednesday to voice their opposition to Senate Bill 277, a proposal to remove personal belief exemptions for childhood vaccinations.
The places where presidential campaigns kick off are almost always laden with symbolism, and for most candidates it is welcome.
Los Angeles Mayor Eric Garcetti on Thursday will announce a new "water conservation engagement campaign" as he presses residents to use less water amid California's worsening drought.
SACRAMENTO — Toilets and faucets sold in California starting next year will have to meet low-flow efficiency standards set by the state under emergency drought regulations approved Wednesday. "In the face of California's current drought, we must use water as efficiently as possible and updating minimum standards for toilets, urinals and faucets is a step in that direction," said Commissioner Andrew McAllister of the Energy Commission in a statement. The commission approved the standards — which apply to toilets and faucets sold and used in residential homes and public bathrooms. Brown met with agricultural, environmental and urban water agency leaders Wednesday to discuss the mandatory water reductions, which will be finalized by the State Water Resources and Control Board next month. Brown opened the final few minutes of the drought meeting to the media and said collaboration is key to addressing the challenges of the drought. Places like San Francisco, which already consume relatively low amounts of water on a per capita basis, would likely have to make smaller cutbacks under the proposed sliding scale of 10-to-35 percent. The San Francisco, Santa Cruz and Monterey water agencies could face a 10 percent cutback under the proposal being weighed by the state water board. The San Francisco Public Utilities Commission has already reduced water use by 7 to 8 percent compared with 2013, meaning under the current proposal, the agency might have to reduce use by an additional 2 to 3 percent. Steve Ritchie, assistant general manager of water for the San Francisco Public Utilities Commission, said even a 2 to 3 percent reduction wouldn't be easy given that the low-hanging fruit is already gone. Ritchie, who attended Wednesday's meetings with Brown in the state Capitol, said urban water agencies seemed to be on board with Brown's conservation mandates. The East Bay Municipal Utility District will vote Tuesday on whether to declare a stage-four drought emergency and trigger more outdoor water restrictions, pursue drought surcharges and begin a public hearing process on penalties for excessive use, which, in extreme cases, could result in the agency turning off the water of repeat water wasters, said agency spokeswoman Abby Figueroa.
David Weidert was sentenced to life in prison for beating, stabbing and strangling 20-year-old Fresno-area resident Michael Morganti in 1980 to hide a $500 burglary.
If you're a public school teacher and you pay your union dues, you get to enjoy whatever salary deal the union negotiates for you.
Legislative Democrats heralded a package of bills they purport to aid and protect undocumented immigrants. Acknowledging the humanitarian concern behind the package, the plan will do little to help immigrants achieve the American Dream if something isn't done to provide middle class jobs. Without them, many immigrants here and those attracted by California 's largesse are subject to a life of poverty.


text:
Report: Astros, Mariners, Yankees interested in Conforto
Bryan Mcwilliam
Mark Brown / Getty Images Sport / Getty
The market for free agent Michael Conforto continues to grow.
The Houston Astros, New York Yankees, and Seattle Mariners are interested in the former New York Mets outfielder, MLB Network's Jon Morosi reports.
At least 3 teams are in on FA Michael Conforto, including his hometown team 👀#MLBNHotStove | @jonmorosi pic.twitter.com/Jlm59RFCfi
— MLB Network (@MLBNetwork) November 29, 2022
Conforto missed the entire 2022 campaign with a shoulder injury but has finished his rehab and is back to 100%, sources told Morosi, who adds the 29-year-old could take a one-year deal to rebuild value and re-enter free agency next offseason.
When healthy, Conforto has been a productive player throughout his career. The left-handed hitter owns a .255/.356/.468 slash line with 132 home runs, 141 doubles, and 396 RBIs in seven seasons, all with the Mets.
The one-time All-Star has also hit more than 27 homers three times in his career and posted an OPS above .900 twice.
The Mets and Chicago Cubs are also reportedly eyeing Conforto.
Marlins' Chisholm named MLB The Show cover athlete
Plan outlined for new Rays ballpark, redevelopment
Braves' Grissom: 'Not trying to fill nobody's shoes' at shor...


text:
Konge i Danmark: Christian 4. 1588-1648

Se også 1631 (tal)

Begivenheder
 Nyboder påbegyndes som et boligkvarter for flådens folk i København
 10. april - en forordning forbyder tiggeri i København
 20. maj - Magdeburg i Tyskland indtages af styrker fra det tysk-romerske rige, der massakrerer de fleste af indbyggerne i en af de blodigste episoder i Trediveårskrigen

Født
 22. februar Peder Syv, folkemindesamler, fødes i Kirke Syv ved Roskilde; han dør i 1702.

Dødsfald
 4. oktober – Sophie af Mecklenburg, dansk dronning (født 1557).

Eksterne henvisninger

31
Artikler om enkelte år

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text:
Jomba Jumps at first Live Performances in 2 Years
Posted On : 1st Aug 2022 Published By : admin
30 August to 11 September 2022
The 24th JOMBA! Contemporary Dance Experience, hosted by the University of KwaZulu-Natal's Centre for Creative Arts, has announced its programme for its first live festival since 2019, which takes place at the Elizabeth Sneddon Theatre, UKZN from 30 August to 11 September 2022.
The theme of this JOMBA! centres around "the (im)possibility of home", and offers dance and theatre fans a treat of 13 days of world-class contemporary dance and performance from both local and international dance-makers. Artists hail from Mozambique, Switzerland, Reunion Island, India, and of course, includes the very best that South Africa has to offer. This edition offers a powerhouse of performances, workshops, after-performance Q & A's, panel discussions, virtual screen dance, and the return of the JOMBA! youth dance platform that continues to support the growth of Durban's young dance communities.
"We are thrilled and relieved to be finally presenting our much-loved festival – live and in-person, while keeping some works and events online to include those not able to attend," says Artistic Director and Curator, Dr Lliane Loots. "This year, through the theme "the (im)possibility of home", we have set out to interrogate a series of dance offerings that negotiate heritage, culture, nostalgia, and identity, which explore a sense of belonging and how this persists, changes, and transforms through time – and what a time (both local and global) for this moment!"
Within this theme, Vincent Sekwati Mantsoe will be honoured as the 2022 JOMBA! Legacy Artist. "This year marks a 30-year history of Mantsoe's career as a dancer and choreographer and we can think of no better way to honour this incredible icon in South Africa's historical dance trajectory than to celebrate with him," says Loots.
There will be a live performance of Mantsoe's new solo work KOMA, the screening of his short dance film CUT (part 1) made during lockdown and his two-year process (2021 and 2022) of working with Durban's FLATFOOT DANCE COMPANY and the long journey to making CUT (part 2) – which will premiere at the festival, and he will present a masterclass.
South Africa's doyens of contemporary dance – the controversial and critical dance-makers – Mamela Nyamza and Nelisiwe Xaba feature with Xaba opening this year's festival in a collaboration with Swiss dance maker Marie-Caroline Hominal in a work intriguingly and simply titled Hominal/Xaba. The deeply interrogated and thoughtful Mamela Nyamza offers her newest work GROUNDED. performed with her son Amkele Mandla, in which she offers us a look into her South Africa where democracy superficially seems to be in a working condition, but actually has small cracks not easy to see.
In partnership with the Goethe-Institut South Africa, JOMBA! will host the inimitable Mozambican dance-maker Edna Jaime in her remarkable solo Um Segundo (One Second).
Fana Tshabalala, the 2019 JOMBA! Mellon Artist in Residence, makes a welcome return with his Broken Borders Arts Project to premiere his latest solo work Zann, which he began creating as part of the 2019 residency.
Three new works by Durban choreographers/dancers – Sandile Mkhize, Tegan Peacock, and Pavishen Paideya will premiere at the festival. All three were given grants to help push their creation of new local work in the JOMBA! EDGE mentored platform.
The JOMBA! YOUTH OPEN HORIZONS (formerly the Youth Fringe), will feature a host of local dance talent at The Stable Theatre.
The virtual offerings include the JOMBA! AFRICAN DIGITAL VOICES, OPEN HORIZONS and an online panel discussion.
In the JOMBA! AFRICAN DIGITAL VOICES platform Mozambican choreographer and dancer Pak Ndjamena, who collaborates with photographer and filmmaker Ivan Barros, has been commissioned to make a screen dance offering One Step at a Time; while Reunion Island's Didier Boutiana and his company SOUL CITY present a dance film titled Le Sol Oblige (The Earth Obliges) a humbling and beautiful look at the relationship of the individual to ideas of home and land, and to community. Mantsoe's Cut (part 1) features online here too.
JOMBA! OPEN HORIZONS (formerly the JOMBA! Fringe) continues to support dance-makers working in film. A jury will select six films to showcase from a call for submissions earlier this year, and the top three will be announced after the viewing.
The festival closes with a virtual conversation between Attakkalari Centre for Movement Arts (Bangalore, India) and artist Simon Senn (Switzerland) looks at the dance work of this amazing centre and the incredible project between Senn and Bharatha Natyam dancer Rohee Oberoi.
There are three open workshops (dancers over 16 only) for dancers and dance-makers, an industry-related session entitled JOMBA! Forging Futures, and the much-valued JOMBA! KHULUMA online writing residency will feature write-ups, interviews and reviews. More details to be announced soon.
Live performances take place at the Elizabeth Sneddon Theatre (UKZN), the Stable Theatre (one performance and free) as well as virtual/online (free) .
Tickets for Elizabeth Sneddon Theatre performances are R80 full price, R65 – students, scholars and pensioners. Booking is through Computicket.
Photo Credits : Val Adamson, John Hogg, Jomba 2022
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Posted in: Arts & Culture, Community Stories, COVID-19, Entertainment, Events, Theatre, UncategorisedTagged : DUrbanTV,Jomba,Jomba 2022,Jomba Dance Festival,tvDUrban,ukzn,UKZN Centre for Creative Arts
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For those who are thinking about locum doctor jobs, there are several things to keep in mind. This can be a rewarding job to some, particularly those who like to travel. Many physicians look at this the top benefit. The work environment and surrounding always change and it offers you the opportunity travel all over the world.
When talking concerning the potential causes of it, you can use various them. In some cases where reflux disease, or GERD, is diagnosed in the individual, the possible causes could vary from physiological dysfunctions for the individual's unhealthy diet. Physiological dysfunctions could be caused by excessive pressure within the stomach or inappropriate activity in the lower esophageal sphincter. The lower esophageal sphincter could be the ring shaped muscular valve that acts since the barrier relating to the esophagus along with your stomach. If this particular muscle is not working or closing properly, the consumer could easily regurgitate the contents of his / her stomach. This is why those with weak lower esophageal sphincter are more likely to be identified as having the reflux disease.
The now limited defense mechanisms isn't competent at overcoming many of these diseases, and must work overtime inside the make an effort to achieve this. Approximately 80% with the defense mechanisms could be the response to Immunoglobin A which is created by the mucosal lining with the digestive system. When the mucosal lining with the intestines just isn't working this may cause autoimmune disease where the immune system attacks parts with the body it is supposed to protect. When the mucosal lining is compromised this limits or ends production of the Immunoglobin A disease fighting antibody and results in contact with many different types of infections.
Many Gastric Bypass patients may resume normal sugar and blood choleseterol levels. Blood pressure problems may dissipate. Sleep apnea and back pain may no longer be problems. The benefits are clear, but so can be the possible complications. Be aware to make a knowledgeable decision before jumping in to the decision to offer the surgery.
Acid reflux disease, also called gastroesophageal reflux disease (GERD) is the result of frequent acid reflux disorder. This is a chronic condition concerning the malfunction with the lower esophageal sphincter (which I'll discuss in just a minute) and aggravated by lifestyle factors offering obesity, certain acidic foods, smoking, alcohol, and usage of large meals.


Sometimes it can be difficult to explain and identify the different features of a typeface. So, let's take a look at the anatomy of typography!
So, I've put together a poster, which I have hanging up in my office! It contains all the significant features of type, pointing out features such as a stem, eye, bowl, counter, arm and so on. I've also included x-height, leading and baseline, which identify features outside of the characters themselves.
I have excluded a few features, but the everyday, common features have been included.
You're welcome to download the file as a reference or bookmark this page.
You can download the image below.
Logo design always throws up all sorts of discussion. Why do some designers charge so much / little for a logo? Why does it take so long to design a logo? What are the benefits of having a logo? And so on.. Well, in this artcile, I'm going to discuss a little bit about the design process when creating a logo. We'll be discussing all sort of things from concepts to final production. Many variables come into play in the process, so I'm going to keep it as general as possible in order to try and communicate the process as best as I can. Here goes!
The brief is extremely important for a logo design. Mainly because what I'm about to create is the face of your company and it's important for me to know as much relevant information about the client's company as I can. So, not only is timeframe, a factor when designing a logo (or anything for that matter), but details regarding your business are just as important.
Business size – sole trader, micro, small, medium, large.
Tagret demographic – almost the most important piece of information. Who are you trying to appeal to?
Product / service cost – who do you cater for, socio-economic wise?
I always begin a logo design with paper, pencil and my A3 sketch book.
Generally, I'll begin with a mindmap, of sorts, or key words about the company, style of the logotype, symbol, colours I may potentially use, the mood of the logo and so on. I believe in writing down as many words to describe what I'm trying to achieve as possible, but I want the words to be accurate to the company, it's beliefs and the target audience.
For my sketches, I very rarely use an eraser, because at this point, the sketches are quite quick and purely encompass an overall style for the logo. The amount of pages I go through for a project really depends on the complexity of the brief. Sometimes it's just a page of sketches, other times 3 - 4 pages. Again, I'm happy to sketch out whatever I feel is relevant to the brief. Whether or not it's going to end up being the final final doesn't worry me at this point in time. Often I'll sketch things which I know won't even be considered, but sometimes they're the link between two very different concepts.
Execution of my sketches isn't hugely important. Some effects and techniques I'll know I can execute better on a computer when I get to that stage.
Once I've completed my sketches, I'll jump into Illustrator and start playing with a few concepts. I sometimes bounce between my computer and sketch book, just to jot down or sketch out a new idea first. For some sketches which I've done quickly by hand, I know how they'll look digitally, but look very different in my sketchbook.
I always design my logos in Adobe Illustrator, regardless of time, who the client is and what they're going to use it for. It is the best application for creating a logo due to the tools available and the accuracy in which it can be produced. Also, as a vector file (which Illustrator handles), I know I'll be able to make the logo as big or as small as I (or the client) want to in the future. I'll begin experimenting with typography, lettering, shapes and scalability of the logo constantly. Scalability is often overlooked by designers and clients alike, as a logo might look fantastic in a large size, but when resized to a smaller size it's unreadble. Having a secondary window open at a smaller scale can also be beneficial.
It's difficult to cover all types of logos in one article, but in general it's important to use as few points as possible in the logo and make it as clean as possible. There shouldn't be any waste.
A business card is a great first impression and while the purpose of a business card has evolved slightly, it's now a very common distribution tool. Many business owners and employees use it as a networking tool and gone are the days of simple, one sided cards being the normal approach to the design.
While many people can't get enough of digital and online information, the business card, along with other print material is still a very commonly printed asset in many countries. And, amazingly enough, standard business card sizes are different all around the world.
So, let's have a look at the standard sizing of business cards. While the differences are only minor, it may effect your job for many reasons. Initially, it's the most important step for business card creation.
I've created a table of standard business card dimensions for different countries around the world, including dimensions (width x height) and bleed dimensions – important for keeping your business card information safely within the card boundaries.
That should give you a better insight as to what dimensions you would like your card to be. Sometimes the standard size isn't necessarily, so it's best to discuss your job before deciding on your sizing.
If you have any further questions about business cards, please feel free to contact me for more information.


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Weybridge residents and visitors alike are enjoying lakeside walks along Broadwater Path, between Grenside Road and Cowey Sale. Its dedication as a public footpath and its new crushed stone surface give year round access to the lakeside – a beautful, tranquil, historic local feature, rich with wildlife.
What many don't know is that the path is essential for the future of the lake itself. Without formal public access, the lake would not qualify for the public funding needed to stop it silting up. Broadwater is a centuries old man made lake, which requires maintenance.
Without dredging, the lake silts and becomes marshland, growing rushes then self-seeded trees. In the 14 years that residents (including PPDRA) pressed for the path, silting got worse at the Greenlands Road end. The middle length also silted badly, until residents raised funds to dredge.
Last year Elmbridge BC contributed a CIL grant, which helped fund some urgent dredging. The Broadwater Conservation Society is now seeking public funding from national sources, and wider local support.
This historic lake is an important part of local heritage. So PPDRA proposes to become affiliated to the Broadwater Conservation Society. To be voted on at our AGM on 13 September.


DJ Pippi & Kenneth Bager's 'La Seranata (Dream Of You)' is a nice summer tune. This collaboration between Ibiza legend, DJ Pippi and Balearic DJ Kenneth Bager was recorded in Ibiza and Denmark, and originally released on 12" vinyl last November on Music For Dreams. DJ Pippi apparently has a reputation as one of Ibiza's best loved, credible house music DJs and holds residencies at Pacha Ibiza, Glitterbox, and the Jockey Club at Salinas beach.
Danish DJ/producer, Kenneth Bager (aka Dr Baker), runs the Music For Dreams label. Kenneth is also the promoter of MFD events at Louisiana Museum (The Guggenheim of Denmark); Coma Club, and the Apple Flower Festival. According to his press, he's been credited with bringing chill out back to Ibiza with a series of events at Sir Rocco, We Love... Sundays at Space and Cafe Mambo.
Now licensed to 3 Beat Records, 'La Serenata (Dream Of You)' is currently available as a digital download, with a vocal version featuring Lilly Wright planned for a full release on 25 September.
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Rolls-Royce's engine test cell, the largest in the world takes shape
Monday 9 September 2019, 1:20 PM
Testbed 80 follows the standard U-shape layout of indoor aviation test facilities, but the size, wall thickness and additional features, such as the equipment for the centre's high-power x-ray, are bespoke. Testbed 80's x-ray equipment will be powerful enough to x-ray a person standing up to six miles away.
A major milestone in the build was recently reached after the twelve augmentor tube pieces were successfully installed. The augmentor tube will direct the exhaust gases from the engine and the testbed bypass air to the back of the facility, where it will be diffused and released through a 37m (121ft) tall exhaust stack.
Fully assembled, the augmentor tube is about as long as half the wingspan of a Boeing 747-B. Each piece of the tube weighs 8 tonnes and are so large they had to be escorted on large trucks through nearby streets when delivered to the site.
Augmentor tubes are a critical part of any aviation testbed. Engine mass flow rates are continuously rising as manufacturers seek to increase thrust and efficiency. As the amount of exhaust gases and bypass air increases in engine test facilities, the design of the facilities is becoming more complex and critical to operational integrity.
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John Jastremski, president and CEO of MDS Aero said, "MDS has a long history of designing test facilities for Rolls-Royce and is at the forefront of research and technology in the narrow field of aeroacoustics, of which there are very few experts."
Constructing the largest aviation test facility of its type in the world with an unprecedented amount of airflow poses a big challenge in this respect and our research and expertise in this area played a big factor in being named the prime contractor on this project.
The new facility will be capable of testing Rolls-Royce's current engines as well as serve as a base for testing the new UltraFan, which is planned for launch in 2025.
Gareth Hedicker, director of development and experimental engineering – civil aerospace, Rolls-Royce said, "Once commissioned, Testbed 80 will be the largest facility of its type in the world. Not only that – it will feature the most advanced testing technology we have ever used.
"Testbed 80 will provide extra capacity as we ramp up production to deliver on our record order book and will be capable of carrying out a full range of indoor testing."
Rolls-Royce opens new £25m Composite...
Korea's Hyundai and Kia to...
Alstom wins £642m Avanti West...
Construction work gets underway on £135m Space Park in Leicester
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First Rolls-Royce powered Airbus BelugaXL enters service
Airbus boss says aerospace giant 'committed' to the UK and plans expansion
Rolls-Royce opens new £25m Composite Technology Facility in Bristol
Spirit Airlines finalises order for 100 Airbus A320neo Family aircraft
Dubai Airshow orders show strong global demand for aircraft
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Home » Uncategorized » Ecuadorean Embassy Speech
Ecuadorean Embassy Speech 74
19 Aug, 2012 in Uncategorized by craig
I spent today inside the Ecuadorian Embassy with Julian Assange, who I am happy to say is both physically and mentally on very good form. I was sitting in the room behind him in a very comfortable leather armchair whilst he made his balcony speech, and I must say I thought the text of it was excellent.
I spoke immediately before Julian, from outside the Embassy. This was my own effort, which I hope provided some valuable context to the persecution of Assange.
I could not help but be struck by the ridiculously excessive police presence – hundreds and hundreds of policemen everywhere. I don't think that the concept of freedom of information can be killed off by the extreme intimidation of a single man, but by Heavens, Hague and Cameron are going to try.
74 thoughts on "Ecuadorean Embassy Speech"
intp1 August 20, 2012 at 09:08
Great Speech, It outshone Assange's really, though I heard his remarks are constrained by Ecuadorian law vis-a-vis political asylum.
John Goss August 20, 2012 at 09:39
Writerman
The whole sequence of events is covered here. First posted by Yonatan.
http://www.nnn.se/nordic/assange/suspicious.pdf
nevermind August 20, 2012 at 10:17
An excellent speech, Craig andjust at the right time. The relevance of it to the assembled Met officers was duly noted, not necessarily by them, they would argue, but in a court of law they could say that they did not know, have never heard of it. They did!
Non of them could possibly get away with raiding an embassy, after having listened to you warning them of the consequences of such actions.
Looks like we all have good reasons now to organise the 'alternative' as someone so aptly said.
I shall meet with a prospective Independent PCC candidate this week. There are 41 of them nationally and a good show in November will be a boost for next years County council elections.
Sorry Charles C., your grumpy cowardly remarks are that of a barrow boy, not a diplomat, whatever your thoughts of Assange this is not relevant.
Who put you up for this Charles?
N_ August 20, 2012 at 10:29
@Jon – I will try to tone down my language as requested, but I am not expecting a response from Charles. I doubt he can do anything other than bilious when he's talking about foreigners HMG doesn't like. Or home-grown oppositionists for that matter.
@expat – Norway did create an oil fund (which they now call a 'pension' fund), but they use hardly any of it for internal industrial development. Most of it's invested abroad. Norwegian economists are trained to think that investing it internally would be ever so dangerous, inviting 'Dutch disease'!
One of the differences with the UK is that in the UK that kind of thing is widely accepted to be the elite's business. Although some of us are old enough to remember the ceremony in which the queen started the oil flowing, we're not supposed to figure out that the oil gets sold and therefore the money must go somewhere. So there's no need for those of us outside the elite to be given a line we can parrot!
It remains true that they run the UK as if it were the British Empire. Look at the school system for one thing.
@Craig – great speech, mate. That it was from the heart came out for me especially when you covered MI6, the media, the need for more people to blow the whistle, and the fake allegations made against whistleblowers, of which you too were a victim.
I think we've all got to keep our anger up. I've seen media articles sneering at David Shayler for cracking up mentally. Got to ask what kind of editor wants such articles and what kind of scribbler types them out. When the Sun sneered at Frank Bruno for having a breakdown, at least they were forced to apologise. But Shayler exposed HMG's crimes in Libya and what they were 'doing a Nelson' to in London. There'll be no apology for him. I hope he recovers.
@ everyone – interesting about Karl Rove in Sweden, eh?
Jon August 20, 2012 at 12:10
@N_, cheers.
@all, safe ground for the BBC, who doesn't have to look far for a wide chorus of mocking and opposition for Assange from the MSM. The Indie and the Guardian, coincidentally, both make references to comedies (Are You Being Served and Monty Python respectively), with the BBC only too happy to echo them both. Very sad indeed.
Sunflower August 20, 2012 at 15:07
What happened in Stockholm was by design, so it seems. But by who and for what purpose has yet to be seen. Sofia Wilen was the catalyst in the early stages, she came in from absolutely nowhere and just happened to have such strong desire to be close to her hero that she eagerly volunteered to help out and managed to end up skin to skin. Sofia has had a very low profile during the consequent time. There is very little information on her, too little.
Then she contacted Anna Ardin and they together went to the police, not to charge him for anything but for asking about advice if they could demand Julian to be tested for VD. Then it all played out from there in the most twisted and wierd forms between the prosecutors and the police and Julian, basically they didn't have anything on him and the prosecutors where just stalling and stalling and stalling. Nothing happened, they had plenty of time to interview Julian in Stockholm if they wanted, but that was not how it was supposed to play out.
The only conclusion one could get out of this is that someone is pulling strings.
me in us August 20, 2012 at 16:50
@Jives – Hi, thanks for looking, and I'm sorry and mystified about your opinion of Michael Moore. I've been following him for years here and I have the greatest appreciation of him and what he does. It's not just respect, it's delight. He's funny and sweet and smart and brave and gets in places others don't. It doesn't even have to be political. Right now he's got a twitter thing going where he tweets when he's going for a walk and people all over put on their shoes and go out and walk with him, wherever they are. They tweet in pictures of things they saw on their walk. He just makes friends and community everywhere. I feel like I'm a friend too so I'll stand up for him here and disagree with you. Best wishes.
@Me In Us: I agree. Part of the problem with some alternative explanation theories is that the lies are said to be so multi-layered, it becomes less about politics and more about philosophy, existentialism and choosing pills from The Matrix. If every challenge to state/corporate power (such as a film director, a whistleblower website or a leaker) is reported in the MSM, then by definition it/they must be a plant, and you should Trust No-one.
I just don't think this is sensible politics, mainly because it is in serious danger of eating itself. By its very rules, holders of such a worldview could easily be accused of being stooges paid to distract people with stuff about Olympic Occult Ceremonies and other nonsense. Occam's Razor seems sensible to apply: greed is wrecking the world, and there are plenty of good people left to challenge it.
Jim Larkin August 20, 2012 at 18:20
The US Center for Constitutional Rights interviewed in this video states that it is generally agreed that in international law, asylum takes precedence over extradition requests.
http://therealnews.com/t2/index.php?option=com_content&task=view&id=767&Itemid=74&jumival=8709
@Jon, thanks. I like questions. I like questioning authority. I like questioning questioners. I want to understand everybody and where they're coming from. A local artist and film critic here, UCSD's Manny Farber, said something I always remember: "I have a great love of the actual." I loved that. I am so big on the truth, the whole truth, and nothing but the truth, and reasoning and jiving together. So I have sympathy with Jives' doubts and questions, I just don't know the rest of it.
I watched a youtube last night, an interview of Chris Paine, the filmmaker who made Who Killed the Electric Car? (* below) and now Revenge of the Electric Car. I had seen it before and I was trying to remember what he said he took from Wikileaks:
http://youtu.be/Xb5y-uSxkCc?t=12m13s
Chris Paine: You know, the most telling thing in this, a lot of people don't know, but if you read the WikiLeaks, there's a lot in WikiLeaks, Saudi Arabia and the U.S. ambassador, about, "You know, we are overstating oil reserves by about 40%. So heads up." And I think this is why the Pentagon is like, "Electric cars are like a good idea, because we need the oil for our supertankers and our airplanes, and let's have a Plan B."
So now the military acknowledges oil depletion, okay, we can try electric cars again. It's not just crimes that WikiLeaks revealed, it's simple world facts we should all know. If you saw Who Killed the Electric Car?, you saw a new, viable alternative to oil get not just killed but disappeared. Every EV-1 got clawed back and shredded, and it wasn't just GM, and the swell battery technology got sold to an oil company that locked it away in a closet. Electric cars came into existence here in part because of a California zero emissions mandate, and then the car and oil companies made the mandate disappear and the cars went with it. Gone, never happened, poof. It set the world back how many years, and we're still doing atrocities everywhere there's oil? How sucky is that? How stupid is that? Pretty sucky, pretty stupid, pretty sad. None of these wars are just or necessary if we could just see clearly and think together. And I think thinking together is fun.
Paine at one point talks about where he's coming from with his films:
http://youtu.be/Xb5y-uSxkCc?t=19m3s
CP: Listen. I majored in international relations, so I was going to be a diplomat or something. And somewhere along the line I learned that no matter how much you argue, you're not going to convince someone of anything, because everyone's already decided what their opinion is. So what can change people's minds are emotions and experiences, and movies have a way of giving people emotions and experiences that don't necessarily need to be argument. And I felt that was a better way to like be persuasive than just arguing all the time.
So, credit to Paine, credit to Moore, credit to Craig, credit to Julian. And credit to Paine's interviewer, whose words end the youtube:
CP: So for a lot of people it's just the experience can change them. Like, "Oh, yeah, I guess I'm behind this." And the argument changes. So I – you know what I'm saying? Like, experience changes people.
DP/30: Yeah. No, the more you know, the less likely you are to be an extreme radical on any side.
CP: Yeah.
So that's my answer to Jives. Thanks all.
(* This is the trailer for Who Killed the Electric Car? — here in Southern California I actually had the chance to lease one. I mean, I saw them myself, they weren't just a theory or a fable: http://www.youtube.com/watch?v=nsJAlrYjGz8 )
@me in us – oh yes, I agree with your approach to questioning. And for the most part, I don't think people should avoid any topics in order to avoid being branded a conspiracy theorist or whatever. I don't know much about electric cars, but I can well imagine they might find it difficult to get to market as a result of corporate chicanery.
But my basic point still stands – there is a brand of political analysis that really ignores the basic Left/Progressive analyses, and wants to see a hidden villain controlling the world, laughing maniacally. Such perspectives are self-fulfilling, since anyone who posits a more complex explanation (such as, how the media tends to follow established power, or how capitalism amplifies greed traits) will get dismissed as a stooge for the system.
(* I'll bookmark your video, will watch when I get a mo – thanks).
Damian Hockney August 21, 2012 at 14:57
As a former member of the now-defunct Metropolitan Police Authority, which held the Met to account, I would have been able to have raised absurd use of resources publicly with those responsible and heard their responses. Now that the authorities have got rid of the MPA and any proper oversight, the forum is not there. Just a part-time committee tacked on to an impotent body, the London Assembly, giving you the opportunity to address questions…to another politician.
Chris23 August 21, 2012 at 18:30
http://www.youtube.com/watch?v=JDaUGB3sjbs
Above is Link To the Australian Doc Film about Wikileaks
Dated JULY 2012
NOT MADE BY BBC
NOT MADE BY FOX
NOT MADE BY CNN
NOT MADE BY CH4
Click on.link
Malaisia August 22, 2012 at 11:40
What impact, if any will Gallaway's comments have? It's pretty clear to me that this is a set up. I may not have all the facts but I can smell a rat – something's not quite right. I even agree with Gallaway's sentiments (that if you have consensual sex, then 3 hours later have sex "half asleep" then go on a couple of dates, it is unlikely that the "half-asleep sex" is rape) but I don't think the way he put it helped Assange. The focus of the debate has moved more towards "was it rape" rather than "is this a set up".
People often say that Assange hasn't been charged and that he has offered to be interviewed in the embassy. However, some say that the Swedish Court don't just want to interview him but arrest him so that he can be charged (i.e. under Swedish law you have to be arrested to be charged). Others point to the fact that Sweden cannot guarantee that he won't be extradited to the US as under Swedish law all extraditions must be looked at on their (individual) merits. I think I have a solution. Why can't Assange reverse the situation (on the promise of no extradition)? He should offer to be tried in absentia from the embassy via web-link with the promise that if he is found guilty he will return to Sweden to serve his sentence (if he really has no charges to answer this should work in his favour). Alternatively, if found guilty, instead of returning to Sweden he could serve the sentence in Britain or even in Ecuador (surely Britain wouldn't deny him safe passage to an Ecuadorian prison cell?).
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Q: Pegar conteudo dentro do iframe Ola,
Utilizo Angular 8.
Preciso pegar o conteudo de dentro do iframe:
O próprio iframe me mostra no console isto:

Mas não se como faço para pegar a informação de dentro dele...
IFRAME

<iframe id="iframe" width="100%" height="400" src="https://dotnetfiddle.net/Widget?Languages=CSharp&projectType=Console&Compiler=Net45&CSharp_CodeBlock=using%20System%3B%0A%09%09%09%09%09%0Apublic%20class%20Classe%20%0A%7B%0A%09public%20double%20Executar%28%29%0A%09%7B%0A%09%09%2F%2F%20Escreva%20o%20c%C3%B3digo%20aqui%0A%09%7D%0A%7D" allowfullscreen="allowfullscreen" frameborder="0"></iframe>

EDIT
Sei que foge da pergunta inicial, mas pensando em ajudar a comunidade deixo uma solução sem iframe para o que eu precisava que era um editor de codigo dentro da minha aplicação, e como nao conhecia outras formas de se fazer, achei que nao existisse algo direcionado para isto.
Pesquisando, eu encontrei o Monaco Editor.

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Q: Absolutely continuous functions that don't have an integrable bound What are some examples of functions that are absolutely continuous, but are not bounded above by any integrable function?
What I am interested in is how the presence of this integrable bound affects the absolute continuity of the associated value function.
An integrable function, is a function which when (Riemann) integrated over its domain, yields a finite number (< $\infty$).
Sorry, I didn't realize how vaguely worded this question is. Here's attempt #2, do there exist $f(x,t)$, where $t$ is a parameter, such $f(x,\cdot)$ is absoultely continuous, but $\not\exists B(t)$, integrable, such that $\sup_{x} |f_{2}(x,t)| < B(t)$ for almost all $t$?

A: Of maps $\Bbb{R} \rightarrow \Bbb{R}$, how about $f(x) = x$, $g(x) = \ln(1+|x|)$, $h(x) = \sqrt{1-x^2}$?
I'm not sure what to make of your second paragraph.  None of these are integrable, so no everywhere larger function is integrable.  ($f$ is the only one that is "close", but its positive part is not integrable, nor is its negative part.)  In fact, the constant function $h:\Bbb{R} \rightarrow \Bbb{R}:x \mapsto 1$ is absolutely continuous, positive, and not integrable, so no everywhere larger function is integrable.


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