text:
\section{Introduction}
Tidal disruption of stars at the centers of galaxies are indicators for the presence of supermassive black holes (SMBHs)
in their nuclei.
Theoretical studies show that when a star passes close to a SMBH it can be tidally disrupted. The
tidal disruption event (TDE) results in about half of the stellar mass falling into the black hole, while the
remaining tidal debris is ejected out from its orbit \citep{rees.1988, ulmer.1999, strubbe.quataert.2009}. This
tidal debris will fall back onto the accretion disk and result in enhanced accretion rates and outflows that
can persist over much longer timescales than the actual TDE (see Bower et al. 2013 and references therein).
Radio jets can be triggered by the infalling debris but the timescale depends on the accretion rates.
In some cases they can be triggered several years after the TDE \citep{Bow11} and will appear as compact emission
associated with the nucleus. In this paper, we analyze late time multi-wavelength observations of the TDE in
NGC~5905 with a special focus on searching for radio jets that may be triggered by the TDE. Late time radio
emission can arise from within the jet itself
\citep{vanvelzen.etal.2011} or from the interaction of the radio jet with the circumnuclear medium
\citep{giannios.metzger.2011}. The resulting blast wave expands into the surrounding circumnuclear gas and later
enters a slower Sedov-Taylor expansion phase which can be detected in radio emission several years after the TDE.
Since most of the TDE host galaxies are at distances of several Mpc \citep{ESKD12, Sax12, cappelluti.etal.2009,
gezari.etal.2009, gezari.etal.2008}, the radio jets will appear as compact nuclear emission. To date only a few TDEs have
been detected in radio emission. Two recent TDEs that were detected in $\gamma$ and X-ray emission showed variable
radio emission that decayed over a timescale of months \citep{bloom.etal.2011, zauderer.etal.2011}. Another source
IC~3599, that was detected in X-ray by {\it ROSAT} showed, however, late time radio emission \citep{Bow13}. This
indicates that late time radio jets or a radio afterglow due to jet-cloud interaction can be observed in TDEs.
Bower et al. (2013) also included NGC~5905 in their study but they did not detect any compact radio source.

\begin{figure}
\includegraphics[scale=0.35,angle=-90]{fig1.eps}
\caption{The first and second segment of the above X-ray light curve were extracted using {\it Chandra} data from Obs-Id~7728
and Obs-Id~8558, respectively. There is no detectable variability
during these observations when the dithering effect is taken into account.}
\label{NGC5905_X-ray_lc}
\end{figure}

\begin{table}
\caption{Details of Observational Data}
\resizebox{\columnwidth}{!}{%
\begin{tabular}{lcccc}
\hline
Wave-& Instrument & Date of Observation & Exposure,Obs-Id \\
length&            &                     & time \\
\hline
X-ray & ACIS-S & 2007-06-07 & 44.95~ks (7728)\\
      &        & 2007-06-09 & 26.95~ks (8558)\\
Radio & GMRT 1.28~GHz & 2011-06-10 & ~2 hours \\
             & VLA FIRST     & May 1997       &  ....    \\
             & VLA 3~GHz     & 2012-06-04 & ~15 min  \\
             & VLA 8~GHz (archive) & 1996-11-03 & ~45 min      \\
 IR    & {\it Spitzer}/IRS & \small 2006-01-16 & SH 30s $\times$ 2 cycles\\
             &                    &                            & LH 60s $\times$ 2 cycles \\
\hline
\end{tabular}
}
\label{obs_detail}
\end{table}

\begin{figure*}
\begin{minipage}{160mm}
\centering
\includegraphics[scale=0.5, angle=-90]{fig2.eps}
\caption{{\it Chandra} image of NGC~5905 in the energy band 0.5-2.0 keV (left panel)
and 2.0-7.0 keV (right panel) is shown. The grey scale numbers are in the units photons~cm$^{-2}$~s$^{-1}$.
The circle of 3.5$^{\prime\prime}$ radius marks the nuclear region of NGC~5905 from which the X-ray spectrum is extracted.}
\label{X-ray_image}
\end{minipage}
\end{figure*}

{\it ROSAT} All-sky survey (RASS) discovered an X-ray flare in
NGC~5905 in 1990. During the X-ray flare the soft X-ray luminosity reached
a peak of $L_X~\sim~6~\times~10^{41}$~ergs~s$^{-1}$ (assuming an absorbed powerlaw
spectral model with $N_H = 1.5 \times 10^{20}$ cm$^{-2}$, a power law index of 4 and distance 47.8 pc)
and decreased below $9 \times 10^{40}$ ergs s$^{-1}$ within 5 months of the
X-ray outburst \citep{BKD96}. Very few cases of X-ray outbursts of
variability amplitude greater than 80 have been observed
\citep{donley.etal.2002, esquej.etal.2007, saxton.etal.2012, maksym.etal.2010}.
Follow-up X-ray observations using {\it ROSAT} and {\it Chandra} show that the X-ray
luminosity of the galaxy declined as $L_X~\propto~t^{-5/3}$, as expected
in the event of tidal disruption of a star near the central BH
\citep{rees.1988, komossa.bade.1999, halpern.gazari.komossa.2004}.
Using the stellar velocity dispersion in the bulge of NGC~5905
\citep[$\sigma = 174.6 \pm 9.0 \rm {km/s}$,][]{Ho.greene.Filippenko.2009}
and the $M_{BH}-\sigma$ calibration \citep{Gultekin.et.al.2009}, the
calculated mass of the nuclear BH in NGC~5905 is $M_{BH} \sim 10^{7}~M_{\odot}$.
This is consistent with the upper limit of $M_{BH} = 10^8~M _{\odot}$
derived by assuming that the 1990 X-ray flare was due to tidal
disruption of a star \citep{halpern.gazari.komossa.2004}.
Hence the nucleus of NGC~5905 may have a SMBH of mass $\sim 10^{7}~M_{\odot}$.

NGC~5905 is a barred spiral galaxy (SB(r)b type) at a distance
of 47.8 Mpc (z=0.011 and H$_0$=73 km s$^{-1}$ Mpc$^{-1}$). It
is classified as a giant low surface brightness (GLSB) galaxy because of its low
surface brightness optical disk (\citealt{kent.1985}; \citealt{sprayberry.etal.1995}).
Like most GLSB galaxies, it is relatively poor in star formation \citep{vanMoorsel.1982}
but it does have a bright bulge and nuclear star formation. H$\alpha$ observations reveal a
circum-nuclear ring of star formation of $\approx$~1~kpc in diameter \citep{mazucca.etal.2008,Com10}.
Ground based optical observations of NGC~5905 classified the nucleus as an HII
or starburst type nucleus (\citealt{G91}, \citealt{Ho95}). However, post-outburst
Hubble Space Telescope/Space Telescope Imaging Spectroscopy (HST/STIS) observations
place it in the low luminosity Seyfert 2 category depending on
the estimated line ratios \citep{gezari.etal.2003}. These observed lines could not be explained
as arising due to photoionization of clouds surrounding the central BH illuminated by the soft X-ray
flare observed in 1990. But at the same time no direct evidence for a non-stellar continuum
was found that could explain the observed line ratios. Thus it is not clear whether there is
an AGN in NGC~5905 but weak AGN activity
cannot be ruled out. Although, in general, AGNs are rare in GLSB galaxies and the BH masses are
lower than those observed in normal galaxies \citep{ramya.etal.2011,Naik10}.

In this study we take a closer look at the late time nuclear emission from NGC~5905. We first examine the 2007 X-ray
observations to constrain the decay of the X-ray flare. We then examine the {\it Spitzer}, {\it Chandra} and radio data to see
if there is a weak AGN in the galaxy (both the {\it Chandra} and {\it Spitzer} data, though archival, are previously unpublished).
Finally we investigate the radio emission using both the VLA 3~GHz data \citep[analyzed as part of][]{Bow13}
as well as low frequency GMRT 1.28~GHz data.  We compare the
3~GHz and 1.28~GHz maps at different resolutions to see if there is a radio jet/afterglow associated with the TDE.
We have also re-analyzed the VLA 8~GHz
archival data of 1996.
Throughout the paper luminosity of the source is estimated assuming
$z=0.0113$ for NGC~5905 and $H_0 = 73~{\rm km~s^{-1}~Mpc^{-1}}$.

\section{Observations and Analysis}
\subsection{{\it Chandra} X-ray observations}

NGC~5905 was observed using the Advanced CCD Imaging Spectrometer (ACIS)
on board the {\it Chandra} X-ray telescope
twice in 2007. Table \ref{obs_detail} gives the details of the observations.
Sometimes large flares are detected in the ACIS
background light curve and if such flares are detected during the observation then
data recorded during the background flares should be
filtered\footnote{{\it Chandra} memo for ACIS background flares}.
No background flares were detected in the ACIS background light curves extracted from
the 2007 observations.

{\it Chandra} 2007 data was used to extract (a)~the X-ray light curve of NGC~5905,
(b)~the image of NGC~5905 in two X-ray energy bands, (c)~the X-ray spectrum
of the central region and (d)~the image of diffuse X-ray emission.
We first examined the source light curve for X-ray flux variability
using the {\it Chandra} task {\texttt{glvary}}. The source light curve
extracted using {\texttt{glvary}} takes into account the variability due to dithering
and optimizes the bin time for the light curve accordingly. A quick look at the light curve
in Figure \ref{NGC5905_X-ray_lc} shows no count rate variability. From the results of
{\texttt{glvary}} we find that the probability that the observed signal is variable is
0.2 and the variability index is 0 implying that no variability was observed during
the 2007 observations of NGC~5905.
\begin{table*}
\centering
\begin{minipage}{155mm}
\caption{Parameters of the X-ray spectrum model}
\resizebox{1.0\columnwidth}{!}{%
\begin{tabular}{lccccccccccc}
\hline
 & & \multicolumn{2}{c}{Component I}&\multicolumn{2}{c}{Component II}& & \\
Model&${\rm N_H}$&$\Gamma$&Norm&kT&Norm&$\chi^2$&dof&$L_{{\rm{x}}(0.5-2~{\rm{keV}})}$&$L_{{\rm{x}}(2-7~{\rm{keV}})}$ \\
&($10^{22}\rm{cm}^{-2}$)& &photons cm$^{-2}$keV$^{-1}$&keV& & & &$\rm{erg~s}^{-1}$&$\rm{erg~s}^{-1}$\\
\hline
wabs(raymond)&$0.015${(fixed)}&--&--&$0.76^{+0.06}_{-0.08}$&$(2.5 \pm 0.6) \times 10^{-5}$&
$13.79$&$13$&$(3.2 \pm 0.2)\times10^{39}$&$(2.5\pm0.4)\times 10^{38}$\\
wabs(pwlw+bb)$^a$&$0.71^{0.48}_{-0.38}$&$3.29^{2.01}_{-1.85}$&$7.34^{2.38}_{-6.19}\times10^{-6}$
&$8.53^{0.04}_{-0.02}\times10^{-2}$&$2.96^{264}_{-2.82}\times10^{-5}$&$12.79$&$11$&
$(3.2\pm0.3)\times10^{39}$&$(7.1\pm4.8)\times10^{38}$\\
wabs(pwlw)$^a$&$0.67^{0.36}_{-0.25}$&$6.79^{2.47}_{-1.71}$&$3.87^{6.44}_{-2.05}\times10^{-5}$&
--&--&$25.74$&$13$& $(3.1 \pm 0.3) \times 10^{39}$ & $(1.1 \pm 0.1) \times 10^{37}$\\
wabs(bb)$^b$&$0.17$& -- & -- &$0.17$&$4.33\times10^{-7}$&$31.44$&$13$ &
$3.11 \times 10^{39}$ & $2.48 \times 10^{37}$ \\
wabs(bb)$^b$&$0.015$ {(fixed)}& -- & -- &$0.22$&
$1.90\times10^{-7}$&$35.41$&$14$ &
$3.06 \times 10^{39}$ & $7.81 \times 10^{37}$ \\
\hline
\end{tabular}
}
\\$^a${Fixing the $\rm{N_H}$ value to the Galactic ${\rm N_H}=1.5\times10^{20}$cm$^{-2}$ gives a bad fit with $\chi^2_{\nu} > 2$}\\
$^b${Reduced $\chi^2$ is greater than 2 and hence no uncertainties on the fitted parameters can be calculated}\\%~~~~~~~~~~~~~}
\label{X-ray_spec_model}
\end{minipage}
\end{table*}

\begin{figure}
\centering
\includegraphics[scale=0.35, angle=-90]{fig3.eps}
\caption{The {\it Chandra} X-ray spectrum of NGC~5905 extracted from the region marked
in figure \ref{X-ray_image} along with the best-fit model (red curve) and the $\chi$
residuals (lower panel). The model is calculated assuming absorbed emission from a hot diffuse gas.
See Table \ref{X-ray_spec_model} for
the model details.}
\label{X-ray_spec}
\end{figure}
Since the source flux did not vary during the two observations of 2007,
we merged the events obtained from both the pointings and made a combined image of NGC~5905 with better
statistics in two energy bands namely 0.5-2.0 keV and 2.0-7.0 keV. Before merging the events,
we matched the aspect solution of
Obs-Id~8558 to that of Obs-Id~7728 using an X-ray point source in the field of view
located at RA~15h~15m~18.254s and Dec~+55$^{\circ}$~32$^{\prime}$~53.71$^{\prime\prime}$.
Since both the observations have
similar pointing offsets of 0.005', the shift is very small,
$\Delta \rm{RA} = {8.63 \times 10^{-6}}{\rm deg}$ and $\Delta \rm{Dec} = -{1.52 \times 10^{-5}}{\rm deg}$,
corresponding to a physical shift in x-direction of -0.06 pixels and in y-direction of
-0.11 pixel. After reprojecting the events to a different tangent point
using the matched aspect solution, combined images in the two energy bands
were extracted using the task {\texttt{fluximage}}. Figure \ref{X-ray_image}
shows the exposure corrected image of NGC~5905 in the two energy bands.
No central peak near or at the location of the optical center is seen in either of the X-ray images.
The observed image of the nuclear region of NGC~5905 is a cluster of bright pixels at the
0.5-2.0 keV energy range. On the other hand NGC~5905 is hardly discernible above the background in the
(2.0-7.0) keV energy image. The number of counts within the 3.5$^{\prime\prime}$ radius nuclear region marked in Figure
\ref{X-ray_image} is 213 and 30 in the 0.5-2.0 keV and 2.0-7.0 keV energy bands, respectively. This
gives a hardness ratio of 0.7 for the nuclear region of NGC~5905.

The spectrum of NGC~5905 is extracted from a circular region of 3.5$^{\prime\prime}$ radius, shown in Figure \ref{X-ray_image}.
We extracted the spectra and responses separately for the two pointings and then co-added them
to get a final combined spectrum. Corresponding background spectra were extracted from a source free region on the CCDs.
The spectra and corresponding responses were extracted using the
task {\texttt{specextract}} and coadded using the task {\texttt{combine\_spectra}}. We grouped the
combined spectrum such that each energy bin has 15 counts. Figure \ref{X-ray_spec} shows the spectrum
of NGC~5905 with the best fit model which describes the observed X-ray spectrum as emission due to hot, diffuse gas.
\begin{figure}
\centering
\includegraphics[scale=0.4,angle=-90]{fig4.eps}
\caption{The H$\alpha$ map taken from the AINUR atlas is plotted in gray scale.
Overlaid on this map are the contours of the X-ray diffuse emission smoothed over 4 pixels.
The contours are 5$\sigma$ to 11$\sigma$ times the noise level in steps of 1$\sigma$. }
\label{X-ray_diffuse_emission}
\end{figure}
To derive the diffuse emission in NGC~5905 we followed the procedure
used in \cite{das.et.al.2009}. The field of view of CCD-Id:~7 was used
and only events in the energy band of 0.5-7.0~keV were included. First, sources
in the field of view were detected using {\texttt{wavdetect}} and then separate
source and background region files for the detected sources were created
using {\texttt{roi}} and {\texttt{splitroi}}. The source count rates were
replaced by corresponding background counts for each source region and an image
for each pointing was created by {\texttt{dmfilth}}. Images and exposure maps,
thus created for each pointing, were combined using the tasks
{\texttt{reproject\_image\_grid}} and {\texttt{reproject\_image}}.
The combined diffuse emission image was first exposure-corrected and then divided by the
exposure map to produce the required flux image. We detected weak, diffuse
emission near the nucleus of NGC~5905. The peak emission has a value approximately
14 times the background emission and this emission lies close to the circumnuclear ring of star formation,
as shown in Figure~\ref{X-ray_diffuse_emission}, where the contours of the diffuse emission
are overlaid on the H$\alpha$ image which is obtained from the Atlas of Images of
NUclear Rings \citep[AINUR,][]{Com10}.
\begin{figure}[t]
\includegraphics[scale=0.4,angle=-90]{fig5.eps}
\caption{{\it Spitzer}/IRS high spectral resolution (SH+LL) spectrum of NGC~5905.
The position of the most prominent emission lines are marked (see Table \ref{IR-line-flux} and text).
}
\label{spitzer_spectrum}
\end{figure}
\begin{table}
\caption{Line fluxes of IR spectral lines}
\resizebox{0.8\columnwidth}{!}{%
\begin{tabular}{lcc}
\hline
Line & Wavelength & Fluxes  \\
element & ($\mu\,\rm{m}$) & ($10^{-14}\rm{ergs\;s^{-1}\;cm^{-2}}$) \\
${\rm [PAH]}$      & 11.25 & $142.00 \pm 1.42$\\
${\rm [Ne II]}$    & 12.82 & $21.64 \pm 3.18$ \\
${\rm [Ne III]}$   & 15.55 & $2.75 \pm 0.39$ \\
${\rm [S III]}$ & 18.71 & $8.49 \pm 1.32$ \\
${\rm [O IV]}$     & 25.89 & $0.57 \pm 0.32$ \\
${\rm [Fe II]}$    & 24.52 & $1.15 \pm 0.34$ \\
${\rm [S III]}$ & 33.48 & $21.06 \pm 2.55$ \\
${\rm [Si II]}$    & 34.8 & $38.16 \pm 3.38$ \\
\hline
\end{tabular}
}
\label{IR-line-flux}
\end{table}

\subsection{{\it Spitzer} mid-infrared observation}
The mid-infrared data were retrieved from the {\it Spitzer} archival
spectroscopic observations (Program ID: IG-A02120140, PI: A. Zezas)
obtained with the infrared spectrograph \citep[IRS,][]{houck.2004}.
The observations were taken with the short-high (SH) and long-high
(LH) modules covering the spectral ranges $9.9-19.6\,\mu$m and
$18.7-37.2\,\mu$m, respectively. The slit width was $4.6^{\prime\prime}$ for SH and $9.0^{\prime\prime}$ for LH.
The observations were reduced following the procedure described in detail by \cite{pereira-santaella.2010}.

Several fine structure lines are observed in the
spectrum along with the $11.3\,\mu{\rm m}$ polycyclic aromatic hydrocarbon (PAH) feature (see Fig. \ref{spitzer_spectrum}). The measured
line fluxes are given in Table \ref{IR-line-flux}. To measure the flux and
equivalent width (EW) of the 11.3$\mu$m PAH feature we used the method of
\cite{hernan-caballero.2011}, which models the feature using a Lorentz function.
There is no indication of the presence of the [NeV] lines
at $14.3\,\mu$m and $24.3\,\mu$m and we put upper limits on their
line fluxes at $0.54 \times 10^{-14}\,\rm{ergs\;s^{-1}\;cm^{-2}}$ and
$0.35 \times 10 ^{-14}\,\rm{ergs\;s^{-1}\;cm^{-2}}$, respectively.
The measured value of the equivalent width (EW) of the $11.3\,\mu{\rm m}$ PAH feature is $1.28 \pm 0.02\,\mu$m
which is typical of high metallicity star-forming galaxies \citep[see][]{hernan-caballero.2011}.

\subsection{Radio Data}
\begin{figure}
\centering
\includegraphics[scale=0.4,angle=-90]{fig6.eps}
\caption{The figure shows the contours of radio continuum emission at 1.28~GHz
overlaid on the 3.6$\mu\,\rm{m}$ IRAC near-infrared
image of the galaxy. The contours are 5,10,15,20 and 25 times the noise level,
which is 0.12~mJy/beam. The beam is elliptical $5.38^{\prime\prime}\times2.21^{\prime\prime}$
and is shown in the bottom left corner. The
radio emission is concentrated about the nucleus within the small but bright
bulge in the galaxy.}
\label{radio_emission}
\end{figure}
\begin{table}[t]
\caption{\bf{Radio Fluxes at different frequencies (with Robust=0)}}
\resizebox{0.9\columnwidth}{!}{%
\begin{tabular}{lccccccc}
\hline
\small $\nu$ & \small Beam  & \small Peak   & \small Noise       & \small Total & \small Fitted  \\
\small (GHz) &              & \small Flux   & \small (mJy/b)  & \small Flux     & \small Size  \\
             &              & \small (mJy/b) &             & (mJy) & \\
\hline
\small 1.28 & \small $5.4^{\arcsec}\times2.2^{\arcsec}$ & 3.84 & \small 0.12 & \small 9.26 & $6.8^{\arcsec}\times4.2^{\arcsec}$ \\
\small 1.42 & \small $5.4^{\arcsec}\times5.4^{\arcsec}$ & 6.44 & \small 0.15 & \small 9.48 & $10.0^{\arcsec}\times7.9^{\arcsec}$ \\
\small 3.0  & \small $2.1^{\arcsec}\times1.4^{\arcsec}$ & 1.04 & \small 0.03 & \small 6.18 & $5.1^{\arcsec}\times3.5 ^{\arcsec}$\\
\small 8.0  & \small $0.26^{\arcsec}\times0.19^{\arcsec}$ & ... & \small \bf 0.030  & \small ...  & ... \\
\hline
\small 1.28$^a$ & \small $4.6^{\arcsec}\times1.7^{\arcsec}$ & 1.32 & \small 0.15 & \small 3.07 & $5.5^{\arcsec}\times2.7^{\arcsec}$\\
\small 1.28$^b$ & \small $11.7^{\arcsec}\times3.8^{\arcsec}$ & ... & \small 0.20 & \small ... \\
\small 3.0$^a$  & \small $1.8^{\arcsec}\times1.2^{\arcsec}$ & 0.42\dag & \small 0.02 & \small 1.87 & ...  \\
\small 3.0$^b$  & \small $1.7^{\arcsec}\times1.0^{\arcsec}$ & 0.18\ddag & \small 0.03 & \small 0.23 & ...  \\
\hline
\end{tabular}
}
~\\
$^a$ uv cutoff 20~k$\lambda$ ~~~~~~~~~~~ \dag left lobe\\
$^b$ uv cutoff 40~k$\lambda$ ~~~~~~~~~~~ \ddag right lobe
\label{radio_obs_detail}
\end{table}
{\bf(i)~1.28~GHz~:~}NGC~5905 was observed during June 2011 in radio continuum
at 1.28~GHz using the Giant Metrewave Radio Telescope (GMRT) located
near Pune, India \citep{ananthakrishnan.rao.2001}.
Nearby radio sources, 1438+621 and 3C~286, were used for
phase and flux calibrations, respectively. NGC~5905 had a two hour scan. The data were
analyzed using AIPS\footnote{Astronomical Image Processing
System (AIPS) is distributed by NRAO which is a facility of NSF
and operated under cooperative agreement by Associated Universities, Inc.} \citep{Greisen03}
and iteratively edited and calibrated until satisfactory gain
solutions were obtained. Low resolution (robust 5) and
high resolution (robust 0) maps were made using IMAGR.
Lower end UV cutoffs of 20~k$\lambda$ and 40~k$\lambda$ (i.e. baselines smaller than 20 or 40~k$\lambda$
were omitted) were applied to see if there was any compact nuclear emission. \\
{\bf(ii)~1.435~GHz~:~}We used the VLA Faint Images of the Radio Sky at Twenty-Centimeters
(FIRST) map\footnote{Faint Images of
the Radio Sky at Twenty-Centimeters} \citep{Becker.et.al.1995} to determine flux at this frequency. The observations were
from the epoch May, 1997. \\
{\bf(iii)~3~GHz~:~} Observations were done in B configuration using the VLA in June 2012.
For further details see Bower et al. (2013). We made robust 0 and robust 5 maps. Lower end UV cutoffs of
20~k$\lambda$ and 40~k$\lambda$ were applied to obtain higher resolution images and to check if there was
any compact nuclear emission.  \\
{\bf(iv)~8~GHz~:~} We used 8~GHz radio data from the VLA archive; the observations
were from the epoch November, 1996 and were taken in the A configuration. We analyzed
the data using AIPS; 1331+305 and 1510+570 were used as flux and phase calibrators, respectively.
The map noise was 29.9$\mu$~Jy/beam, where the beam is 0.28$^{\prime\prime} \times 0.19^{\prime\prime}$,
and is consistent with the earlier analysis of \cite{komossa.dahlem.2001}. We did not detect any compact emission
in either robust=0 or robust=-5 (highest resolution) maps. The 5$\sigma$ upper limit to any radio
afterglow is thus 150$\mu$~Jy and is consistent with the $5\sigma$ upper limit given by
\cite{komossa.dahlem.2001}

\section{Results}
\subsection{Long term behavior of X-Ray Luminosity of NGC~5905}
The best fit model (emission due to hot diffuse gas) to the 2007 X-ray spectrum yields
the X-ray flux of the source as $f_{\rm{x}}=(1.5 \pm 0.1)\times10^{-14} \rm{erg~s}^{-1}\rm{cm}^{-2}$
in the energy band of $0.3-8.0~\rm{keV}$ (also see Table \ref{X-ray_spec_model}).
We also tried other models, the details of
which are presented in Table \ref{X-ray_spec_model}. The powerlaw model with variable
$N_H$ gives a very high value for the powerlaw index. A purely powerlaw model with
absorption column density fixed to galactic value ($N_H=1.5\times10^{20} \rm{cm}^{-2}$)
gives a very poor fit. We also tried an absorbed blackbody model with variable and fixed $N_H$
values but both the models give poor fits. We also tried to model the spectrum as
thermal bremsstrahlung but the resultant fit was very poor. For comparison,
the 0.1-2.4 keV X-ray luminosity of NGC~5905 during the 2007
{\it Chandra} observations is a factor of $\sim 200$ less than the luminosity
observed during the peak of the X-ray flare in 1990.

\begin{table}
\caption{X-ray Luminosity}
\resizebox{0.8\columnwidth}{!}{%
 \begin{tabular}{cc}
 \hline
 \small Time & \small $L_{\rm x}$ (0.1-2.4)keV \\
 \small (year) & \small ($\rm{erg~s^{-1}}$) \\
 \hline
 1990.53$^a$ & $(6.45 \pm 2.29) \times 10^{41}$ \\
 1990.54$^a$ & $(8.05 \pm 2.05) \times 10^{41}$ \\
 1990.54$^a$ & $(1.17 \pm 0.18) \times 10^{42}$ \\
 1990.54$^a$ & $(1.28 \pm 0.21) \times 10^{42}$ \\
 1990.54$^a$ & $(1.17 \pm 0.17) \times 10^{42}$ \\
 1990.54$^a$ & $(1.67 \pm 0.25) \times 10^{42}$ \\
 1990.54$^a$ & $(1.52 \pm 0.23) \times 10^{41}$ \\
 1990.97$^a$ & $< 2.52 \times 10^{41}$ \\
 1991.04$^a$ & $< 2.80 \times 10^{41}$ \\
 1993.55$^a$ & $(1.97 \pm 0.29) \times 10^{40}$ \\
 1996.89$^a$ & $(1.15 \pm 0.17) \times 10^{39}$ \\
 2002.76$^b$ & $(4.95 \pm 0.99) \times 10^{39}$ \\
 2007.44$^c$ & $(4.40 \pm 0.10) \times 10^{39}$ \\
 \hline
 \end{tabular}
}
~\\
$^a$ \cite{li.etal.2002} \\ $^b$ \cite{halpern.gazari.komossa.2004}\\ $^c$ This work \\
\label{xlum}
\end{table}

\begin{figure}[t]
\includegraphics[scale=0.4,angle=-90]{fig7.eps}
\caption{Figure plots log$L_{\rm x}$ in the 0.1-2.4 keV energy range as a function of log$(t-t_D)$
where $t_D=1990.36$. Table \ref{xlum} gives the values of time of observation and $L_{\rm x}$
used in this plot. Data to derive these values have been taken from
\cite{li.etal.2002} (open circle), \cite{halpern.gazari.komossa.2004} (filled circle), the 2007 luminosity being
derived from this work and adjusted to the (0.1-2.4) keV energy band (open square). The solid line
represents the best fit slope of $(-1.23 \pm 0.03)$; the dashed line
represents the expected (-5/3)~slope of the TDE model expected decline in
$L_{\rm x}$ as a function of time and the dotted line represents the constant luminosity
due to nuclear star formation.
}
\label{long-term-X-ray-lc}
\end{figure}

Figure \ref{long-term-X-ray-lc} shows a plot of the long term variation in the observed X-ray
luminosity of the source since the 1990 X-ray flare.
The luminosities used in this plot are listed in
table \ref{xlum}.
It is clear that the X-ray luminosity estimated from the 2002 and 2007 {\it Chandra} observations
are comparable within errors. We note here that, for the {\it ROSAT} observations, we use the
observed count rates given in \cite{li.etal.2002} to estimate the flux of NGC~5905 using
WebPIMMS\footnote{http://asc.harvard.edu/toolkit/pimms.jsp} and assuming a blackbody spectrum of
$kT = 0.06$. The declining X-ray luminosity is best fit with $L_{\rm x} \propto (t-t_D)^{\gamma}$ where
$t_D=1990.36$, $\gamma = -1.23 \pm 0.03$ plus a constant luminosity due to nuclear star formation.
The dashed line in figure \ref{long-term-X-ray-lc}
is the predicted theoretical TDE curve with $\gamma=-5/3$ used to explain the 1990 X-ray flare
of NGC~5905 \citep{li.etal.2002,halpern.gazari.komossa.2004} and the dotted
line represents the constant luminosity due to
nuclear star formation. The $\gamma$ we get from our fitting depends on the value of $t_D$ which is fixed; hence
the real $\gamma$ value might be much closer to $-5/3$ than indicated here.

\subsection{Diffuse X-ray Emission}
We have detected faint diffuse X-ray emission (when the bright patch
of pixels at the optical location of NGC~5905 are subtracted) from within the bulge,
about $2^{\prime\prime}$ from the galaxy center. The AINUR H$\alpha$ image
of NGC~5905 shows the presence of a central ring of nuclear
star formation \citep{Com10}. Figure \ref{X-ray_diffuse_emission}
is an overlay of the X-ray diffuse emission contours on this H$\alpha$ map.
There is no strong spatial correlation between the H$\alpha$ and the
diffuse X-ray emission. Therefore this diffuse X-ray emission could
be due to gas infall associated with the large scale bar in the galaxy
and the formation of the nuclear ring.

\subsection{No AGN signatures in X-Ray, IR or Radio emission}

The X-ray image of NGC~5905 (Figure \ref{X-ray_image}) is a cluster of
bright pixels. This cluster of bright pixels are clearly visible in
the 0.5-2.0 keV energy band and are very faint in the 2.0-7.0 keV energy
band.
From the photon counts within the 3.5$^{\prime\prime}$ radius marked in figure~\ref{X-ray_image}
the hardness ratio of the source is $\sim$0.7. The estimated source luminosity in the 0.5-8.0~keV
energy band is $\sim 4.1 \times 10^{39}$ erg~s$^{-1}$. Presence of an AGN is expected if
the X-ray image shows a bright point source at the optical center with a hardness ratio greater
than 0.8 and a source luminosity greater than $3 \times 10^{42}$~erg~s$^-1$ \citep{bauer.etal.2004}.
It is also noted here that the Raymond model for emission from hot diffuse gas
gives the best fit to the X-ray spectrum indicating that the observed X-ray flux
is probably all due to the nuclear star formation.

The {\it Spitzer}/IRS mid-infrared spectrum does not show any [NeV] lines at 14.3 or $24.3\,\mu$m
which are expected if the galaxy hosts an AGN. The measured
[OIV]$25.89\,\mu$m/[NeII]$12.81\,\mu$m ratio ($\simeq 0.02$)
indicates that the nuclear emission of this galaxy is completely
powered by star formation \citep[see][]{pereira-santaella.2010,tommasin.et.al.2010}.
To constrain the AGN contribution, if any, we can compare various line
ratios with the EW of the $11.3\,\mu{\rm m}$ PAH features using the
diagnostic diagrams of \cite{tommasin.et.al.2010}. Accordingly we calculate
upper limits for [NeV]14.32 $\mu$m/[NeII]12.82 $\mu$m at 0.025 and for
[NeV]14.32 $\mu$m/[SiII]34.8 $\mu$m at 0.014. The line ratios for [OIV]/[NeII]
and [NeIII]/[NeII] are $0.02 \pm 0.01$ and $0.12 \pm 0.02$, respectively.
Using the estimated line ratios and the value of EW of the $11.3\,\mu{\rm m}$
PAH feature in Figures 4a and 4b of \cite{tommasin.et.al.2010} we conclude that
the IR flux is nearly 100\% dominated by the starburst emission.
Indeed the semi-analytical models suggested by \cite{tommasin.et.al.2010}
estimates 5.6\% AGN emission at 19~$\mu$m using the [OIV]/[NeII] line ratio
which is consistent with the $<$34.6\% AGN emission suggested by the
upper limit on [NeV]/[NeII] line ratio.
The bright 11.3$\mu$m PAH feature and the [NeII] line
at $12.81\,\mu$m also indicate that there is high star formation
in the nuclear region of the galaxy. From the star forming region (SFR) calibration
given in \cite{diamond.2012} based on the [NeII] line we obtain
a nuclear SFR (for a Salpeter IMF) of $2.3\,M_{\odot} {\rm yr}^{-1}$,
in good agreement with the estimate of \cite{mazucca.etal.2008}
using H$\alpha$ observations. Using the correlations between SFR
and the soft X-ray luminosity of \cite{Pereira-Santaella.et.al.2011}
we get an expected 0.5-2.0 keV X-ray luminosity of
$\sim 4\times10^{39}\rm{erg~s^{-1}}$ consistent with the measured
X-ray luminosity (see Table \ref{X-ray_spec_model}) leaving no excess
X-ray emission which can be associated with a central Seyfert 2 type AGN.

The absence of radio emission in the 8~GHz VLA radio map also points
to the absence of an AGN. The flux density of radio emission from AGNs
does not fall as sharply with increasing frequency as SFRs \citep{condon.1992}. Hence if the compact radio core was due to
an AGN, we would have observed some emission at 8~GHz as well.

\cite{gezari.etal.2003} observed NGC~5905 in the optical using the HST/STIS
which has a narrow slit size of $0.1^{\prime \prime}$ and hence detected
narrow emission lines from the nuclear region of the galaxy. But they
did not detect any broad Balmer line emission. Furthermore, the spatial profile
of the HST acquisition image obtained by them also does not indicate any AGN-like
unresolved point source in the nucleus. Thus no evidence for an AGN
is found from X-ray, Optical, IR or radio data. We infer that any AGN present in
NGC~5905 is very weak, as also indicated by a low total X-ray luminosity
(see Table \ref{X-ray_spec_model}), and rule out the possibility that the
X-ray flare of 1990 in this galaxy observed by RASS was a result of large-amplitude variability
in the Seyfert nucleus.

\begin{figure*}[t]
\begin{minipage}{170mm}
\centering
\includegraphics[width=7cm]{fig8a.eps}
\includegraphics[width=7cm]{fig8b.eps}
\includegraphics[width=7cm]{fig8c.eps}
\includegraphics[width=7cm]{fig8d.eps}
\caption{Panel showing the inner 10$^{\prime\prime}$ nuclear star forming ring in H$\alpha$ emission and radio emission at
1.28, 3.0 and 8.0 GHz. All the images are centered at the optical center of the galaxy (15:15:23.321, +55:31:02.51).
Clockwise from top left (a) H$\alpha$ image from the AINUR survey (Comeron et al. 2010); (b) The 1.28~GHz GMRT  radio
image made with robust=-5 which gives the highest resolution map. The peak flux is 1.81 mJy/beam where the beam
is 4.97$^{\prime\prime} \times$1.63$^{\prime\prime}$ and the map noise is  87.6~$\mu$Jy/beam. (c) the 3~GHz VLA image
made with robust=-5. The peak flux
is 0.74~mJy/beam where the beam is 1.84$^{\prime\prime} \times$1.17$^{\prime\prime}$ and the map noise is
81.45~$\mu$Jy/beam. Note that the center of
the circum nuclear ring coincides with the location of the peak emission in the GMRT 1.28~GHz map. (d)
The VLA 8~GHz map made with robust=0 (as it has more emission than robust=-5) and convolved with a 1$^{\prime\prime}$ beam to
obtain a smoothed map. Note that the emission appears to be associated with the circum nuclear ring.}
\label{panel}
\end{minipage}
\end{figure*}

\subsection{Radio emission at 1.28~GHz and 3~GHz~:~the circumnuclear star formation}
At all resolutions in the GMRT maps, the 1.28~GHz radio emission
shows strong nuclear emission but no extended structure that could be associated with large scale jets or
disk emission (see Figure~\ref{radio_emission}). The source structure and flux density are
similar to that of the FIRST image (Table~\ref{radio_obs_detail}).
The NVSS map has a flux density of 20.1~mJy which is significantly higher
than both the FIRST and GMRT maps. But this may be due to the larger NVSS beam
(45$^{\prime\prime}$) which picks up more of the extended diffuse emission.
To see if there is any compact nuclear emission in the 1.28~GHz radio image, we made a high resolution
map using the imaging parameter, robust=-5 (Figure~\ref{panel}(b)). The emission peaks close to the galaxy nucleus and
has a value of 1.81 mJy/beam where the beam is 4.97$^{\prime\prime} \times$1.63$^{\prime\prime}$ and
the map noise is 0.088~mJy/beam. But it is offset
from the optical center by approximately an arcsecond. The emission is also extended. Hence we could not detect
any compact emission that could be a radio afterglow associated with the TDE at 1.28~GHz.

At 3~GHz, however, the 1.28~GHz nuclear emission breaks up into a double lobed structure
(Figure~\ref{panel}(c)) that could be either due to a weak AGN or emission
from the limb brightened edges of a nuclear ring. Since there is a circumnuclear star
forming ring in the galaxy ((Figure~\ref{panel}(a)), a nuclear ring is more likely. The size and orientation
of the ring matches the high resolution 1.28~GHz radio morphology. The size is also similar to the H$\alpha$
image of the circumnuclear ring. All these factors suggest the 3~GHz emission is mainly due to circumnuclear
star formation. Using the total flux at 1.28 and 3~GHz (Table~\ref{radio_obs_detail}) we obtain a spectral index of
$\alpha~=~0.5$ where $S_{\nu}\sim{\nu}^{-\alpha}$. This is typical for both radio jets and
star formation. However the high resolution radio geometry suggests that star formation is more likely.

At 8~GHz we obtained only patchy emission. To see if there was any extended emission that was not picked up by the
small beam, we smoothed the 8~GHz map (robust=0, lower resolution) to 1$^{\prime\prime}$
resolution (Figure~\ref{panel}(d)). No compact
emission that could be due to a TDE was detected, but some patchy emission close to the noise limit is seen.
It is probably associated with the star forming ring.

We used the radio flux at 1.4~GHz in the FIRST map (Table~\ref{radio_obs_detail}) to estimate the star formation rate in
the nuclear region using the relation $\rm{SFR}=(L_{1.4}/4\times10^{21}~WHz^{-1})~M_{\odot}yr^{-1}$\citep{condon.1992}.
We obtain a value of 0.61~${\rm M_{\odot}yr^{-1}}$, which is lower than the value
that we obtained from the {\it Spitzer} spectrum, 2.3~$\rm{M_{\odot}yr^{-1}}$ and from the H$\alpha$
observations of the nuclear ring, 2.6~$\rm{M_{\odot}yr^{-1}}$ \citep{mazucca.etal.2008}. This could be
because the SFR derived from radio continuum assumes the presence of massive
stars which are usually associated with supernova that emit synchrotron radiation. However, NGC~5905 is a
giant LSB galaxy and in such systems massive stars may not be common.

One question that arises is whether the TDE could have triggered the nuclear star formation through gas
shocked by radio jets. This is
unlikely as the ring has an inner diameter of 0.5$^{\prime\prime}$ to 1$^{\prime\prime}$. Even with velocity
close to speed of light ($c$),
the time required to reach such radius is of the order of several $\sim100$~yrs. However, the
higher nuclear mass density makes a TDE more probable.

\subsection{Nuclear radio emission~:~Is there a TDE radio afterglow?}

As mentioned in the introduction, TDEs can result in enhanced
SMBH mass accretion rates which can result in the formation of radio jets or
outflows from the nucleus. They will appear as relatively weak but
compact radio emission associated with the nucleus. One of the main goals of this study
is to detect such a radio afterglow from NGC~5905. To search for compact emission we
applied 20-0 and 40-0 k$\lambda$ UV range cutoffs (i.e. only UV
wavelengths greater than 20 or 40 k$\lambda$ were included) to both the 1.28~GHz
and 3~GHz maps (see Table~\ref{radio_obs_detail} for fluxes). The 1.28~GHz 20~k$\lambda$ map
has a peak coincident with the center
of the 3~GHz ring (Figure~\ref{panel}). But when a 40~k$\lambda$ cutoff
is applied, no compact emission remained - which suggests
that the 20~k$\lambda$ 1.28~GHz peak was probably due to diffuse emission associated
with star formation and not compact emission associated with the TDE.
The 3~GHz images with 20-0 and 40-0~k$\lambda$ UV range cutoffs
(Figure~\ref{panel} b and c) show a nice ring but no compact nuclear emission.
Thus both the 1.28 and 3~GHz radio data (both obtained after the epoch 2010) do not show any emission that
could be associated with the TDE. But the map noise at 1.28~GHz and 3~GHz constrains the
radio afterglow to lie between 0.62~mJy and 0.09~mJy (3$\sigma$ limits), respectively. We did not
detect any emission in the VLA 8~GHz (1996) archival data  as well.
Instead the map noise gives a 5$\sigma$ limit of 0.15~mJy for an 8~GHz afterglow.

\section{Conclusion }
\noindent
{\bf 1. X-ray emission:} From the 2007 {\it Chandra} X-ray spectrum of NGC~5905 we conclude that the observed X-ray emission
at that epoch can be fully accounted for as emission from a hot diffuse gas probably present due
to the nuclear star formation. \\
{\bf 2. No evidence for an AGN:} No evidence for an AGN is found from X-ray, IR or radio observations.
The predicted 0.5-2keV X-ray luminosity obtained from the IR SFRs compares well with the observed  X-ray luminosity.
The non-detection of the high excitation [NeV] lines together with the observed EW of the 11.3~$\mu$m PAH feature and
mid-IR line ratios indicate that the mid-IR emission of this galaxy is fully arising from star formation
activity. According to the \cite{tommasin.et.al.2010} semi-analytical models, the [OIV]/[NeII] line ratio
suggests an AGN contribution of only 5.6\% to the total IR flux at 19~$\mu$m. Also radio emission at 8~GHz is absent.
Therefore the STIS data \citep{gezari.etal.2003} can imply only a very weak AGN in NGC~5905. \\
{\bf 3. Circumnuclear star formation:} The 3~GHz image of the galaxy shows a double lobed structure the size of
which is similar to the H$\alpha$ image of the circumnuclear ring. The size and orientation of this structure
matches with the 20~k$\lambda$ 1.28~GHz radio morphology. Thus the 3~GHz radio emission is likely due to the circumnuclear
star forming ring in NGC~5905. \\
{\bf 4.~No Confirmed Radio Afterglow~:~} We did not detect any compact emission associated with the TDE at
1.28~GHz, 3~GHz or 8~GHz. Such emission could arise from a radio jets triggered by the TDE.  Upper
limits to any flux associated with a radio afterglow can be given by 3$\sigma$ (where $\sigma$ is the map
noise) and is 0.62~mJy at 1.28~GHz, 0.09~mJy at 3~GHz and 0.09~mJy at 8~GHz.

{\bf 5. Long term X-ray luminosity:} The long term X-ray luminosity shows a decline after the 1990 X-ray flare
detected by RASS. This decline follows the expected decline if the 1990 X-ray flare was due to TDE. The
observed luminosity decline is well modeled as $L_{\rm x} \propto (t-t_D)^{\gamma}$ where $t_D$ is the year 1990.36,
$\gamma = -1.23 \pm 0.03$ plus a constant luminosity due to nuclear star formation.

\section*{Acknowledgments}
We thank Sebastien Comeron for giving us the AINUR image of the nuclear ring in NGC~5905,
M. Pereira-Santaella for his help with the {\it Spitzer}/IRS spectra, S. Tommasin for help
with their semi-analytical models of IR emission lines and S.~Komossa for very useful
discussions regarding this work. We also thank G.C. Bower for his very useful comments
which have improved this work and for sharing the 3~GHz EVLA data used in the work.
A.A.-H. is party funded by the Spanish Plan National grant AYA2012-31447.
We thank the GMRT staff for help in observations.
The GMRT is operated by the National Center for Radio Astrophysics of
the Tata Institute of Fundamental Research. This work has used VLA 3~GHz and 8~GHz archival data of
NGC~5905. It has also used the NRAO VLA FIRST image and the 8~GHz NRAO VLA Archival data of NGC~5905.
The NRAO (National Radio Astronomy Observatory) is a facility of the National Science Foundation operated
under cooperative agreement by Associated Universities, Inc.
This research has made use of data obtained from the
{\it Chandra} Data Archive and the {\it Chandra} Source Catalog, and software provided by the
{\it Chandra} X-ray Center (CXC) in the application package CIAO. This work is based [in part] on
observations made with the {\it Spitzer} Space Telescope, which is operated by the Jet Propulsion Laboratory,
California Institute of Technology under a contract with NASA.
This research has also made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the
Jet Propulsion Laboratory, California Institute of Technology, under contract with the
National Aeronautics and Space Administration.

\bibliographystyle{spr-mp-nameyear-cnd}

redpajama_set_name: RedPajamaArXiv


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text:
No demonstrations after elections - Gambia's Jammeh orders
Ismail Akwei with AFP
Gambia's incumbent president Yahya Jammeh who is a candidate in the country's December 1 presidential elections said on Tuesday that demonstrations will not be allowed after the elections.
"There is no reason to protest because the election cannot be rigged, and in this country, anyway, we do not allow demonstrations," he said on the last day of campaigning that saw thousands rally behind opposition leader Adama Barrow.
"Nothing will happen, this is not the first time we organized elections," Jammeh told thousands of his supporters in Banjul.
There is no reason to protest because the election cannot be rigged, and in this country, anyway, we do not allow demonstrations.
"They (the opposition) will not win," he added.
The main opposition leader elected by seven opposition party coalition, Adama Barrow, has urged President Jammeh to be calm when he loses the election.
Adama Barrow and Mamma Kandeh, the third candidate, campaigned hard to win the votes of 886,578 electorates at 1,422 polling stations in 53 constituencies in the seven administrative regions of the country.
The winner of the election will enjoy a five-year term as president.
The small West African nation with less than two million people will also hold legislative and local elections in April 2017 and April 2018 respectively.
Click here to follow our news coverage on The Gambia
Exiled Gambian president accused of rape by beauty pageant
Gambian soldiers sentenced for plotting to overthrow president Barrow
Gambia signs oil deal with BP [Business Africa]
Yahya Jammeh
Mauritania's new president takes office on August 1, victory validated
Mauritania elections: vote counting underway
Malawi protests turn violent after disputed election
Mauritania elections: official campaign kicks off [Morning Call]
Cyril Ramaphosa officially takes office, but who becomes his next deputy?
Malawi's president makes final plea for re-election in tight race

redpajama_set_name: RedPajamaCommonCrawl


But he reiterated that the region's aspirations were not comparable to the secessionist agenda that has provoked a constitutional crisis in Spain. Independence-minded Veneto easily met a turnout threshold to validate the vote set by Mr Zaia, with some 60% of the region's four million voters casting ballots.
The movie was a flop but learned her critical acclaim for her performance. It is a traditional Sindhi ceremony. "Their bonding is divine!" Read Also: Mommies-to-be Esha Deol, Soha Ali Khan, Celina Jaitley, Sunidhi Chauhan enjoy their baby glow Esha had been following a healthy diet, and practiced yoga nearly every day, through these nine months to stay physically fit.
General Gatot Nurmantyo, commander of Indonesia's Armed Forces (TNI), was about to board an Emirates flight last Saturday when the airline informed him that the United States authorities had denied him entry, Reuters reported. The same conference past year, also hosted by Dunford, saw senior military chiefs from 43 nations, including Indonesia, flocking to Washington to discuss the challenges posed by worldwide terrorism.
In a revealing few minutes in a larger interview with Maria Bartiromo of Fox Business Network , Trump repeatedly said he might not have been elected without his use of social media and explained why he finds it such an appealing outlet. Describing John Kelly's reaction to Congresswoman Frederica Wilson telling reporters that Trump said La David Johnson "knew what he signed up for", Trump says to Bartiromo that the Chief of Staff "actually couldn't believe it".
But then, yesterday, he was dragged into the sordid spectacle of Trump's fight with a congresswoman and the grieving family of La David Johnson , the Army sergeant who was killed in Niger earlier this month. Video of the speech contradicted his recollection. He followed up with a tweet Friday calling Wilson a "wacky Congresswoman." Wilson said. "This is incredible".
Fortunately for her, no train was approaching the tracks at the time of the incident. Shocking footage shows him waving to a friend standing on the platform across from the woman before shoving her onto the tracks. Suddenly, out of the blue, the man pushed her over the edge at the Yuen Long station, according to the South China Morning Post . The cleaner was rescued from the tracks and taken to Pok Oi Hospital.
He told Sky News: "We hung around outside for a little while. we didn't know what to do, what was going on". "There were police cars arriving, there was a helicopter, police dogs, armed police stood all around the bowling alley". The leisure park where a gunman is holding hostages inside a bowling alley. Ms Mjeshtri said she was eventually allowed to leave after police moved her vehicle to a safer place.
Shortly after the Palestinian unity government was formed, Israeli Prime Minister Benjamin Netanyahu reacted with similar sentiments, conditioning the acceptance of the deal on recognising Israel and disarming Hamas , which Israel considers a terrorist organisation.
Wesley Mathews, 37, was arrested for suspected child endangerment for the treatment of his daughter, Sherin, after claims he sent her outside alone in an alley before she was reported missing on October 7. Dogs had been used in the search of the girl and police went door-to-door looking for any information on her whereabouts. They towed in the family's two SUV and a minivan, in search "potential evidence".
Typhoon Lan , a storm with an eye 50 miles wide, is expected to lash parts of Japan with intense wind and rain, the country's meteorological office has warned. Commercial aviation is taking another hit this weekend as hundreds of flights have been canceled in and out of Japan while the nation prepares for the onslaught of Typhoon Lan .
The North's official Korean Central News Agency reported on Saturday that the chief of the North's mission to the United Nations made the request in a letter to the president of the Security Council on Friday. "I don't think there's any evidence that what the Russians did changed enough votes, or any votes", Carter told The New York Times in an interview published on Saturday.
But the Timberwolves , without any more timeouts, swiftly found Wiggins who skipped through the Thunder defence to launch a long-three that banked in on the buzzer. Russell Westbrook scored 15 of his 31 points in the fourth quarter. Anthony scored 23 points, and Paul George had 14 points on 6-for-20 shooting.
The EC just said polling in the western state would be held before December 18. The former finance and home minister also claimed the Election Commission will be "recalled" from its "extended holiday" after the Gujarat government has announced all "concessions and freebies".
Terrorists on Sunday hurled a grenade at the residence of a National Conference (NC) leader in Pulwama's Tral, Jammu and Kashmir (J&K). A woman was shot dead and another injured by Jaish-e-Mohammed militants in a south Kashmir village on Sunday, police said.
Later addressing the press, Swaraj highlighted the issues discussed by JCC. Speaking at the fourth Joint Cooperation Committee (JCC) in Dhaka , External Affairs Minister Sushma Swaraj said both countries will continue fighting terrorism, radicalisation and extremism.
The device burned his groin but failed to explode, saving the lives of the other 289 people aboard. But the 30-year-old Muslim filed a lawsuit with a Colorado federal court this week in which he claims his constitutional rights have been violated by the US Justice Department.
John Mapozi and Sam Gitau who were members of Senator Susan Kihika's media team. Nakuru County Senator Susan Kihika said that three of the five people believed to be in the chopper (names withheld) were members of her communication team. National Disaster Management Unit Deputy Director Pius Masai said the team is in place facilitating the search and rescue operations alongside the Kenya Navy.
Tillerson made clear that the comments delivered in Wednesday's speech-where he also criticized Chinese financing that he said leaves developing countries saddled with debt-weren't off-the-cuff. The Secretary of State said India and China both have risen over the past decades to become global powers. "And yet, the Obama administration chose to be less overt in calling out China and in highlighting it as a point of convergence for U.S.
Clinton said. But after discovering that majority were, she said that "Bill and I looked at each other and said 'well, we gotta go'". Hillary , who is a former first lady due to the presidency of her husband Bill Clinton , had to face the reality that she lost to Donald Trump who has proved to be a contentious figure.
Germany have won two of three meaningful knockout games though, including a 4-3 win in the third-place match in Mexico in 2011. The Carlos Amadeu coached Brazil has impressed with its game both in the creative and striking zones where the likes Lincoln, Paulinho and Brenner have excelled alongside the play-maker Alan.
President Donald Trump will not attend the event, but will appear by video to thank people who have contributed to the relief effort. The five former presidents will all be on hand at the One America Appeal event, being held in College Station , Texas, where the George H.W.
In September, during the meetings of worldwide leaders at the UN General Assembly, President Trump and Secretary Guterres had addressed the subject, a priority for the White House . Although President Trump praised Secretary Guterres for the initiatives taken to improve the functioning of the organization his administration wants to reduce the U.S.
Jenkins' body was found September 10 in a walk-in freezer at a Rosemont hotel where she had been attending a party. The authority said, there is "no evidence that indicates any other conclusion". Jenkins in the hotel kitchen. "The majority of people at the party included close friends and even relatives of Ms. Jenkins". The lawyers said the death-scene photos were shown to the family by Rosemont police during a meeting Thursday to update the family on the death investigation.


(CNN) — Arizona's attorney general proposed arming one principal or employee at each school to defend against attacks such as the recent Connecticut school massacre.
"The ideal solution would be to have an armed police officer in each school," Attorney General Tom Horne said in a news release Wednesday. But budget cuts have limited the number of Arizona schools with "school resource officers" on campus, he said.
A shooter, armed with a semiautomatic rifle and two other guns, on December 14 killed 26 people — including six faculty members and 20 young students — at Sandy Hook Elementary in Newtown.
Horne compared the plan to the FAA's program adopted after the September 11, 2001, attacks to arm airline pilots.
A school would be invited to send the principal "or another designee" to "training in the use of firearms and how to handle emergencies such as that which occurred in Newtown," Horne's release said. Horne's office would oversee the free training with help from sheriffs, he said.
"The designated individual (no more than one per school) would then be authorized to keep a firearm locked in a secure place, and would have adequate communication to be alerted to an emergency in any part of the school," the release said.
Several Arizona sheriffs have joined in to support the proposal, Horne said.
Legislation to allow it will be introduced by the Republican leader in the state House, he said.


text:
Tarleton's second half rally falls short against Eastern Michigan
TSU Sports Information
LAS VEGAS – A furious second half comeback by Tarleton fell short in a 65-59 loss to Eastern Michigan in the Texans second and final game at the South Point Classic on Monday.
The Texans rallied from a 13-point halftime deficit to retake the lead 59-57 with 3:06 remaining after Iyana Dorsey drained a 3-point shot from the left key. Eastern Michigan then closed the game on an 8-0 scoring run as the Texans went without a field goal the rest of the way.
Tarleton held the Eagles scoreless for more than seven minutes in the fourth quarter to claw its way back in its final nonconference game this season.
A pair of jump shots from senior Alexa Hoy and a finish in the paint by Kandyn Faurie pulled the Texans within one point at the 4:06 mark of the final frame and set up Dorsey's go-ahead triple.
Hoy finished with a team-high 16 points while Dorsey (14 points) and forward Lucy Benson (12 points) also scored in double figures. Benson ignited the Texans' offense in the third quarter, finishing twice at the rim and converting 3-4 foul shots to pull Tarleton within seven points entering the final frame. Dorsey also scored seven of her points in the third frame.
Benson, a 5-11 senior from Kennedale, Texas, tied her career high in rebounds with nine to lead the Texans on the glass.
The Texans trailed by as many as 15 points in the first half as the team got off to a slow offensive start. Tarleton shot 6-24 from the field in the game's opening 20 minutes and connected just twice from long range. Tarleton took advantage of its opportunities at the foul line to stay in the contest early, as the team went 12-14 at the charity stripe in the first half and was 20-24 for the game.
Tarleton came out of the second half reenergized defensively as well. The Texans held the Eagles to 26 points out of the intermission and limited the Eagles to 10-30 shooting and no made 3-point field goals. The Eagles 36 percent shooting clip was the lowest opponent shooting percentage Tarleton has allowed against a Division I opponent this season.
The Eagles took advantage of extra opportunities at the rim, though, to stay in front of Tarleton. The Texans were outscored 16-4 in second chance points and 38-18 inside the paint.
The Texans' nine turnovers were the team's second-lowest single game mark of the season.
Hoy and fellow guard Jayci Morton each finished with four rebounds while Emily Cunningham led Tarleton in assists with four in her third game back from a brief injury absence. Callie Boyles swatted her 18th and 19th shots in 20 minutes off the bench and now leads the Western Athletic Conference in blocks per game (2.7).
The loss dips Tarleton's overall record to 3-6. Eastern Michigan, which lost to Gonzaga in its first game of the tournament on Sunday, is now 4-3. The Texans remain winless away from Wisdom Gym.
The team will now break for 18 days before beginning its debut season in the WAC with a pair of games against Grand Canyon on Jan. 8-9 in Phoenix. Tarleton's WAC home-opener is scheduled for Jan. 15 against California Baptist.


text:
Saint-Cyr-sur-Mer ist eine französische Gemeinde mit  Einwohnern (Stand ) an der Mittelmeerküste (Côte d'Azur) im Département Var in der Region Provence-Alpes-Côte d'Azur. Die Gemeinde liegt zwischen Bandol und La Ciotat im Westen des Départements.

Die Gemeinde Saint-Cyr-sur-Mer besteht aus dem Hauptort Saint-Cyr, dem Haupthafen Les Lecques und dem kleinen Hafen La Madrague. Sie gehört zum Kanton Le Beausset im Arrondissement Toulon.

Geschichte

Das Gebiet von Saint-Cyr-sur-Mer ist seit prähistorischen Zeiten besiedelt. Einen Höhepunkt erlebte die Siedlung in romanischer Zeit, aus der zahlreiche archäologische Befunde stammen, die heute im romanischen Museum Tauroentum zu besichtigen sind.

Im Jahr 1825 löste sich Saint-Cyr-sur-Mer von La Cadière-d'Azur und wurde eine selbständige Gemeinde.

1913 wurde anlässlich der Inbetriebnahme des ersten Wasserleitungsnetzes in Saint-Cyr auf dem Grande Place eine verkleinerte Replik von Bartholdis Freiheitsstatue aufgestellt.

Wirtschaft
Die Hauptwirtschaftsfaktoren sind Landwirtschaft und Tourismus. Der Ort gehört zum Weinbaugebiet Bandol (Côtes de Provence AOC Bandol).

Verkehr
Saint-Cyr-sur-Mer verfügt über eine Ausfahrt an der Autoroute A 50. Ein Bahnhof an der Bahnstrecke Marseille–Ventimiglia existiert ebenfalls. Der Flughafen Marseille ist etwa 64 Kilometer entfernt.

Gemeindepartnerschaften
Saint-Cyr-sur-Mer ist mit dem südbadischen Denzlingen und Città della Pieve in Italien partnerschaftlich verbunden, die beide auch untereinander durch Partnerschaften verbunden sind.

Weblinks

 Offizielle Website der Gemeinde Saint-Cyr-sur-Mer (französisch)
 Website des Tourismusbüros Saint-Cyr-sur-Mer (französisch, englisch, deutsch)

Einzelnachweise

Ort in Provence-Alpes-Côte d'Azur
Weinbauort in Frankreich

redpajama_set_name: RedPajamaWikipedia


FRAMINGHAM, Mass.—S2 Security, a provider of IP-based access control and video management and mobile security management systems, has put the monitor on the network with its Magic Monitor, a move that S2 CEO John Moss says "fundamentally changes the value proposition of a security management system.
FRAMINGHAM, Mass.—Network-based integrated security system provider S2 Security on July 17 launched its S2 Global product. Designed for customers with multiple dispersed facilities, S2 Global connects multiple devices in security management systems and video management systems.


text:
Francisco Paulo Mignone (São Paulo, 3 de septiembre de 1897 — Río de Janeiro, 19 de febrero de 1986), pianista, compositor, director de orquesta y pedagogo, es una de las figuras más significativas de la música clásica brasileña, y uno de los más importantes compositores brasileños después de Heitor Villa-Lobos. En 1968 fue elegido como compositor brasileño del año.

Mignone fue un compositor versátil, dividiendo su producción por igual entre canciones solistas (canções), piezas de piano, obras instrumentales de cámara, orquestales y corales. Además, escribió cinco óperas, ocho ballets y bastante música para películas.

Biografía
Hijo de un padre inmigrante italiano y flautista, Alferio Mignone, Francisco comenzó con él su aprendizaje musical, antes de tomar lecciones de piano con Silvio Lema. En sus inicios en el mundo musical brasileño, a los 10 años, adquirió cierta notoriedad en su distrito tocando en el estilo «choro». Como pianista y director de orquesta, a los 13 años, ya había adquirido cierta fama componiendo y tocando bajo el seudónimo de Chico Bororo, manteniendo estas actividades aparte de su formación musical formal. Luego, en 1913, entró en el Conservatorio de São Paulo, donde estudió armonía y composición con Savino de Benedictis, y piano con Agostinho Cantú. En 1920 continuó su formación en el Conservatorio de Milán (Italia) con Vincenzo Ferron. Mignone volvió a São Paulo en 1929 para enseñar armonía, y en 1932 se trasladó a Río de Janeiro para enseñar dirección orquestal en el Instituto (Conservatorio) música nacional.

Sus obras pueden dividirse en tres períodos de composición. Sus primeras obras muestran la influencia italiana y la sensibilidad romántica de su formación en Milán, con una gran influencia sobre todo de Ottorino Respighi. Una pieza orquestal de su primera ópera de este período inicial fue estrenada en Río de Janeiro en una gira de Richard Strauss con la Orquesta Filarmónica de Viena, en 1923, estando Mignone al frente de la orquesta.

Una segunda etapa, la más larga, es fuertemente nacionalista en el sabor, influido por su antiguo maestro de escuela, el escritor y musicólogo Mário de Andrade, y con su compatriota Heitor Villa-Lobos, ya anciano, como referente. Mignone utiliza el folk y las melodías populares y las formas de su Brasil nativo como base para sus composiciones, con algunas reminiscencias de la música africana. (Andrade dijo en una ocasión: «En la música italiana, Mignone sería uno más entre los ricos y numerosos escolares, a la que no añadiría nada. Aquí, será de indispensable valor.») Desde 1929 hasta 1960 sus obras están fuertemente caracterizadas por el nacionalismo, una etapa en la que compuso piezas como las Fantasias Brasileiras (1929/36), o los ballets Maracatu de chico rei (1933) y Leilão (1941). Su obras solistas para voz y piano de ese momento le valieron la aclamación por su expresión de los estilos musicales brasileños, como el choro, la modinha, y las «valsas» (valses) que recuerdan a las serenatas.

La música de Mignone se caracteriza por su lirismo, colorido instrumental y estilo improvisatorio. La mayor parte de sus primeras obras son tonales, como es típico de la música popular y folk, aunque más adelante su carrera tendrá ramificaciones politonales, atonales y seriales. A finales de los años 1950, Mignone se alejó de la música nacionalista y se volvió hacia las entonces tendencias actuales en la música académica de concierto, componiendo obras como su Concierto para piano (1958), que muestra su habilidad y bravura en la instrumentación. Mignone era capaz de escribir en una variedad de estilos y sus obras de comienzos de los años 1960 y en adelante destacan por su eclecticismo, siendo difícil encontrar cualquier otra característica unificadora. Sin embargo, regresó a la escritura nacionalista en sus últimos años.

A los 83 años Mignone se casó con Maria Josephina, con quien a menudo interpretó duetos al piano, y que sigue siendo intérprete de su música hasta el día de hoy.

Catálogo de obras

Referencias
 Gerard Béhague: "Francisco Mignone". New Grove Dictionary of Music and Musicians.

Enlaces externos
 Sobre Francisco Mignone (con MIDI scores)

Compositores de música clásica de Brasil del siglo XX
Compositores de ópera de Brasil
Compositores para piano
Nacidos en São Paulo


text:
Customer Highlight — Buffalo Clover
Looking for something new to move you? Check out the new Buffalo Clover album – Low Down Time, available from Nashville's Palaver Records.
http://www.youtube.com/watch?v=FEIayWZiKIw
Buffalo Clover is a rare plant that grows in the wake of stampeding buffalo. It is also the name of one of Nashville's most eclectic bands. Fronted by songstress Margo Price, the group draws its inspiration from true roots music. Price and her husband/co-writer, Jeremy Ivey, formed the band after meeting in Nashville in 2008. Their styles range from underdog gypsy punk to Motown boxcar blues, Vaudevillian acid rock to train wreck folk. Their songs are unique yet familiar with a lyrical craft rarely present in popular music.
The musical line up of the group has changed over the years, but the core has remained the same. With the meeting of guitar/banjo player, Matt Gardner in 2009, the band added the talents of another great writer and performer. The three have played with a rotating cast of musicians. Bass player, Jason White has also been an important part of the group since 2008.


text:
HomeTrout in the Classroom
What is Trout in the Classroom?
Trout in the Classroom, now know as the Classroom Aquarium Education Program (CAEP) in California (encompassing Trout in the Classroom, Steelhead in the Classroom, Salmonids in the Classroom, and the Salmon and Trout Education Program) is a relatively simple program and has been a huge success so far. Basically, teachers set up an aquarium and incubate trout eggs in their classroom, under the guidance of a Trout in the Classroom coordinator. Together, they ensure that all of the equipment has been purchased and is assembled by January. The teacher and students are responsible for daily maintenance and observation of the eggs, while the coordinator is responsible for obtaining permits and delivering the eggs. The final result is an aquarium full of trout fry that is released into a pre-approved body of water during a class field trip. Trout in the Classroom is an extremely rewarding program for everybody involved, whether student, teacher, or mentor.
Trout in the Classroom (TIC) programs have been in place all across the country for more than 20 years. In California SIC/TIC was started through the efforts of the Diane Higgins and Dave Armocido in 1989. The program was designed specifically for teachers who want to incorporate more environmental education into their curriculum and need outside help. It gives DVFF members the opportunity to get involved with their local schools, while teaching kids about water quality, aquatic life, and other environmental issues. The program is also supported by Trout Unlimited, with additional info here.
There are as many opportunities as there are schools and teachers in your area. Nevertheless, it is extremely important that you find a teacher who is very excited about the idea and will work with you throughout the entire process; the teacher who chooses to undertake this program is the secret to its success. The Diablo Valley Fly Fishers has successfully administered a program for a number of years. They currently have over a dozen classes participating in the program.
What are the requirements for setting up a program?
Interested teacher.
Permission of school principal.
A letter of agreement with the school, including a transportation arrangement for field trips.
Attending the required "In-Service" class program held by the California Department of Fish & Game, East Bay Regional Parks and the local fly clubs. Check the CA DFG website for more information.
Instructions for teacher to follow in setting up classroom aquarium.
Aquarium and other related equipment.
How can I get funding?
Trout in the Classroom projects are partially funded by Diablo Valley Fly Fishers (DVFF). The equipment costs around $360.00 for the "Cool Works Chiller System." Schools will often have small grants available for programs like Trout in the classroom. Other sources of funding include:
Energy Companies
National Fish and Wildlife
Parent Teacher Associations
Contra Costa County Fish & Wildlife Committee
Alameda County Fish & Wildlife Committee
What equipment do we need?
Trout in the Classroom aquarium system starts with a 10 gallon tank and a Cool Works Ice Probe. The outer foam box and added insulation for the aquarium allow the water temperature to be maintained at 48 degrees to 56 degrees.
What permits do I need before I start?
Permit from DFG for transporting and having the eggs is required and must be filed out and returned upon release of the fry.
Permit for a field trip to the local lake for release and permission to release from the local governing body (EBMUD, East Bay Regional Parks or CA DFG).
DVFF members are encouraged to participate in this program!
TIC in the News
Tassajara Hills Elementary
Participating Schools:
Buena Vista Elementary, Contra Costa Christian School, Del Rey Elementary, Dorris-Eaton, Donald Rheem Elementary, Lafayette Elementary, Windermere Elementary, Los Medanos Elementary, Mt. Diablo High School, John Baldwin Elementary, Sequoia Middle School, Springhill Elementary, St. Mary's Primary, Stanley Middle School, Tassjara Hills Elementary, Valley Middle School, Willow Cove Elementary, Hidden Hill Elementary, Washington Manor, Montevideo Elementary, Walnut Creek Elementary and Charlotte Woods.
Interpretive Center
Los Vaqueros Interpretive Center
Gerry Ng
8 San Pedro Place
geraldjng@gmail.com


text:
Niederweimar ist ein Ortsteil der Gemeinde Weimar (Lahn) im mittelhessischen  Landkreis Marburg-Biedenkopf und Sitz der Gemeindeverwaltung.

Geschichte

Ortsgeschichte
Die älteste bekannte schriftliche Erwähnung von Weimar erfolgte unter dem Namen Wimare im Jahr 1138/39. Dabei ist aber nicht klar, ob es sich um Ober- oder Niederweimar handelt. Die älteste bekannte Erwähnung von Niederweimar unter dem Namen Niderwimere stammt aus dem Jahr 1320.

Ein erster Ausbau des Dorfes setzte nach dem Bau der Main-Weser-Bahn und der Einrichtung eines Haltepunktes an dieser Bahnlinie ein. Nach dem Zweiten Weltkrieg wurden am Hang des Weinberges (südliches Ende des Marburger Rückens) in verschiedenen Phasen Neubaugebiete erschlossen.

Hessische Gebietsreform (1970–1977)

Gemeinsam mit Oberweimar und Allna war Niederweimar im Zuge der Gebietsreform in Hessen am 1. Februar 1971 auf freiwilliger Basis Gründungsort der neuen Großgemeinde Weimar (Lahn), die inzwischen aus zwölf Ortsteilen besteht. Für Oberweimar wurde wie für die übrigen Ortsteile von Weimar ein Ortsbezirk mit Ortsbeirat und Ortsvorsteher eingerichtet. Als Verwaltungssitz wurde der Ortsteil Niederweimar bestimmt.

Staats- und Verwaltungsgeschichte im Überblick
Die folgende Liste zeigt die Staaten, in denen Niederweimar lag, und deren nachgeordnete Verwaltungseinheiten, denen es unterstand:

 vor 1567: Heiliges Römisches Reich, Landgrafschaft Hessen, Amt Marburg
 ab 1567: Heiliges Römisches Reich, Landgrafschaft Hessen-Marburg, Amt Marburg
 1604–1648: Heiliges Römisches Reich, strittig zwischen Landgrafschaft Hessen-Darmstadt und Landgrafschaft Hessen-Kassel (Hessenkrieg), Amt Marburg
 ab 1648: Heiliges Römisches Reich, Landgrafschaft Hessen-Kassel, Amt Marburg
 ab 1754: Heiliges Römisches Reich, Landgrafschaft Hessen-Kassel, Amt Kaldern und Reitzberg
 ab 1806: Landgrafschaft Hessen-Kassel, Amt Kaldern und Reitzberg
 1807–1813: Königreich Westphalen, Departement der Werra, Distrikt Marburg, Kanton Lohra
 ab 1815: Kurfürstentum Hessen, Amt Kaldern und Reitzberg
 ab 1821: Kurfürstentum Hessen, Provinz Oberhessen, Kreis Marburg
 ab 1848: Kurfürstentum Hessen, Bezirk Marburg
 ab 1851: Kurfürstentum Hessen, Provinz Oberhessen, Kreis Marburg
 ab 1867: Königreich Preußen, Provinz Hessen-Nassau, Regierungsbezirk Kassel, Kreis Marburg
 ab 1871: Deutsches Reich,  Königreich Preußen, Provinz Hessen-Nassau, Regierungsbezirk Kassel, Kreis Marburg
 ab 1918: Deutsches Reich, Freistaat Preußen, Provinz Hessen-Nassau, Regierungsbezirk Kassel, Kreis Marburg
 ab 1944: Deutsches Reich, Freistaat Preußen, Provinz Kurhessen, Landkreis Marburg
 ab 1945: Amerikanische Besatzungszone, Groß-Hessen, Regierungsbezirk Kassel, Landkreis Marburg
 ab 1946: Amerikanische Besatzungszone, Hessen, Regierungsbezirk Kassel, Landkreis Marburg
 ab 1949: Bundesrepublik Deutschland, Hessen, Regierungsbezirk Kassel, Landkreis Marburg
 ab 1974: Bundesrepublik Deutschland, Hessen, Regierungsbezirk Kassel, Landkreis Marburg-Biedenkopf
 ab 1981: Bundesrepublik Deutschland, Hessen, Regierungsbezirk Gießen, Landkreis Marburg-Biedenkopf

Gerichte seit 1821
Mit Edikt vom 29. Juni 1821 wurden in Kurhessen Verwaltung und Justiz getrennt. In Marburg wurde der Kreis Marburg für die Verwaltung eingerichtet, und das Landgericht Marburg war als Gericht erster Instanz für Niederweimar zuständig. 1850 wurde das Landgericht Marburg in Justizamt Marburg umbenannt. Nach der Annexion Kurhessens durch Preußen 1866 erfolgte am 1. September 1867 die Umbenennung des Justizamtes in Amtsgericht Marburg. Auch mit dem Inkrafttreten des Gerichtsverfassungsgesetzes von 1879 blieb das Amtsgericht unter seinem Namen bestehen.

Bevölkerung

Einwohnerstruktur 2011
Nach den Erhebungen des Zensus 2011 lebten am Stichtag dem 9. Mai 2011 in Niederweimar 2382 Einwohner. Darunter waren 63 (2,6 %) Ausländer. Nach dem Lebensalter waren 411 Einwohner unter 18 Jahren, 999 zwischen 18 und 49, 495 zwischen 50 und 64 und 477 Einwohner waren älter. Die Einwohner lebten in 1050 Haushalten. Davon waren 324 Singlehaushalte, 300 Paare ohne Kinder und 309 Paare mit Kindern, sowie 93 Alleinerziehende und 241 Wohngemeinschaften. In 195 Haushalten lebten ausschließlich Senioren und in 741 Haushaltungen lebten keine Senioren.

Einwohnerentwicklung

Historische Religionszugehörigkeit

Historische Erwerbstätigkeit

Kultur und Sehenswürdigkeiten

Ortskern
Der kreisrunde Dorfkern von Niederweimar liegt an einer ehemaligen Furt durch die Allna im Verlauf der alten Weinstraße, die von hier bis nach Goßfelden über den Marburger Rücken und westlich an Marburg vorbei verlief. Von der Weinstraße zweigte hier eine Talstraße nach Marburg ab. In der Mitte des Ortskerns liegt die Alte Kirche, die heute als Kulturveranstaltungszentrum genutzt wird, nachdem sie in den 1970er Jahren durch das neue evangelische Gemeindezentrum ersetzt wurde.

Vereine
Ein sportliches Angebot in Niederweimar bietet der TSV Niederweimar mit den Abteilungen Fußball, Tischtennis, Turnen und Badminton. Vom Schützenverein wird Luftgewehr-, Luftpistole- und Bogenschießen angeboten. Außerdem gibt es in Niederweimar einen Verein für Musik, den Männergesangverein, zwar singen die Männer zurzeit nicht mehr, aber es gibt auch einen gemischten Chor und einen Kinderchor für die Kleinsten, welche vom MGV als Träger unterhalten werden. Auch eine Freiwillige Feuerwehr existiert im Ort.

Infrastruktur
Durch Niederweimar führt die Bundesstraße 255 sowie die Main-Weser-Bahn.
Regionale Bedeutung erlangt Niederweimar durch das Freizeitgebiet Weimarer See mit seinem Badestrand und seiner Wasserskianlage.

Literatur

Weblinks

 Ortsteil Niederweimar. In: Webauftritt der Gemeinde Weimar.

Einzelnachweise

Ort im Landkreis Marburg-Biedenkopf
Geographie (Weimar (Lahn))
Ehemalige Gemeinde (Landkreis Marburg-Biedenkopf)
Gemeindeauflösung 1971


text:
STLC with `Nat` and `Bool` with simple **concept parameters**:

*   **Concepts** contains only names with types

    ```
    C := <empty>
       | CDef C

    CDef ::= concept Id
               f1 : T1
               f2 : T2
               ...
               fn : Tn
             endc
    ```

*   **Models** consist of concept-names definitions:

    ```
    M := <empty>
       | MDef M

    MDef ::= model Id of Id
               f1 = t1
               f2 = t2
               ...
               fn = tn
             endm
    ```

*   **Types** are STLC types with _concept parameters_:

    ```
    T ::= Nat
        | Bool
        | T -> T    (function)
        | C # T     (concept parameter, C is a concept)
    ```

*   **Terms** are STLC terms with _model applications_:

    ```
    t ::= true
        | false
        | n          (natural constant)
        | pred t
        | succ t
        | mult t t
        | if t then t else t
        | t t
        | \x:T.t
        | t # m      (model application)
        | \c#C.t     (c is a concept parameter of concept C)
    ```

### cpSTLCa Coq Definitions

#### Syntax

```coq
Inductive ty : Type :=
  | TBool : ty
  | TNat  : ty
  | TArrow : ty -> ty -> ty        (* T1 -> T2 *)
  | TConceptPrm : id -> ty -> ty   (* C # T *)
.

Inductive tm : Type :=
  | tvar  : id -> tm               (* x *)
  | tapp  : tm -> tm -> tm         (* t1 t2 *)
  | tabs  : id -> ty -> tm -> tm   (* \x:T11.t12 *)
  | tmapp : tm -> id -> tm         (* t1 # M *)
  | tcabs  : id -> id -> tm -> tm  (* \c#C.t1 *)
  | tcinvk : id -> id -> tm        (* c.f *)
  | ttrue  : tm
  | tfalse : tm
  | tif : tm -> tm -> tm -> tm     (* if t1 then t2 else t3 *)
  | tnat   : nat -> tm             (* n *)
  | tsucc  : tm -> tm              (* succ t1 *)
  | tpred  : tm -> tm              (* pred t1 *)
  | tplus  : tm -> tm -> tm        (* plus t1 t2 *)
  | tminus : tm -> tm -> tm        (* minus t1 t2 *)
  | tmult  : tm -> tm -> tm        (* mult t1 t2 *)
  | teqnat : tm -> tm -> tm        (* eqnat t1 t2 *)
  | tlenat : tm -> tm -> tm        (* lenat t1 t2 *)
  | tlet   : id -> tm -> tm -> tm  (* let x = t1 in t2 *)
.
```

#### Typing

```coq
Inductive namedecl : Type :=
  | nm_decl : id -> ty -> namedecl   (* f : T *)
.
Definition namedecl_list : Type := list namedecl.

Inductive conceptdef : Type :=
  | cpt_def : id -> namedecl_list -> conceptdef   (* concept Id NameDefs endc *)
.
Definition conceptsec : Type := list conceptdef.

Inductive namedef : Type :=
  | nm_def : id -> tm -> namedef   (* f = t *)
.
Definition namedef_list : Type := list namedef.

Inductive modeldef : Type :=
  | mdl_def : id -> id -> namedef_list -> modeldef (* model Id of Id NameDefs endm *)
.
Definition modelsec : Type := list modeldef.

Inductive program : Type :=
  | tprog : conceptsec -> modelsec -> tm -> program
.

(** [tycontext] is a typing context: a map from ids to types. *)
Definition tycontext := partial_map ty.

(** AVL map from [id] to [ty]. *)
Definition id_ty_map := id_map ty.

(** Concept type *)
Inductive cty : Type := CTdef : id_ty_map -> cty.

Definition find_ty := mids_find ty.

(** AVL map from [id] to [tm]. *)
Definition id_tm_map := id_map tm.

(** Model type *)
Inductive mty : Type := MTdef : id -> id_tm_map -> mty.

Definition find_tm := mids_find tm.

(** Concept symbol table is a map from concept names
    to concept types [Ci -> CTi]. *)

Definition cptcontext : Type := partial_map cty.
Definition cstempty : cptcontext := @empty cty.

(** Model symbol table is a map from model names
    to model types [Mi -> MTi]. *)

Definition mdlcontext : Type := partial_map mty.
Definition mstempty : mdlcontext := @empty mty.

```

#### Checking Concepts, Models, and Programs

```coq
(** Concepts *)

Definition concept_defined (st : cptcontext) (nm : id) : Prop.
Definition concept_defined_b (st : cptcontext) (nm : id) : bool.

Inductive type_valid (st : cptcontext) : ty -> Prop.
Fixpoint type_valid_b (st : cptcontext) (t : ty) : bool.

Definition concept_welldefined (st : cptcontext) (C : conceptdef) : Prop.
Definition concept_welldefined_b (st : cptcontext) (C : conceptdef) : bool.

Definition concept_has_type (cst : cptcontext) (C : conceptdef) (CT : cty) : Prop.
Definition concept_type_check (cst : cptcontext) (C : conceptdef) : option cty.

(** Terms *)

Inductive ctxvarty : Type :=
  (* type of term variable [x : T] -- normal type *)
| tmtype  : ty -> ctxvarty
  (* type of concept parameter [c # C] -- concept name *)
| cpttype : id -> ctxvarty
.

Definition context : Type := partial_map ctxvarty.
Definition ctxempty : context := @empty ctxvarty.

(** Typing rule *)
Inductive has_type : cptcontext -> mdlcontext -> context -> tm -> ty -> Prop.

(** Models *)

```

### Notes

Our simple concepts do not contain type parameters/members,
that is why types do not depend on _concept parameters_,
they can only include _concepts_
(like type `C # T` of term `\c#C.t`).

redpajama_set_name: RedPajamaGithub


I want to live in a beautiful western country but it is impossible for me because I don't have money nor a degree. I really don't like being here in my country at all. I will do labor jobs in factories or shop and so on, my English is also good, I want to live in the USA, but problem is how do I get there without money and what visa they will give me, I don't understand, there is no support from my parents and anyone, they are uneducated and don't understand much, I m from India, there are many Indians who live there but they are highly educated and some are rich, but it is impossible for me due to my life circumstances there are many people who live in the USA from around the world who do multiple jobs and earn well, I have it online, I can do the same, factory job or at shop or any local job, I can drive uber too, but problem is how do I get there, I really want to be in the USA, And I m a good person with no bad background at all, I don't like my country at life here at all.
Hello all! So, I need help if anyone can assist me with this. I've been going to the UK since mid December and I've gone 3 times as of today, totaling 9 days all together. My question is for how much longer can I go for the remainder of the year? I am planning on going in July for as long as I can possibly go for... Also, once I am there, can I apply for a visitor visa or will I need to come back home? and if so, how long would I need to wait to return?
Best answer: We will have almost a million unpapered non-citizens this year. San Francisco and Sacramento should take at least 200 thousand of them. They have said they welcome them. Democrats are only sending them to small Republican towns.
Best answer: The Gulf countries get away with a lot of stuff that most others wouldn't. But in general someone is only deported when they've refused to leave voluntarily, thus proving that they don't play well with authorities. So while they may be allowed back in on a sponsored immigration visa, they remain a high risk for any visa type that involves them eventually returning to their home country. As for your friend, yeah, the UAE and its neighbors are pretty capricious about certain things and because they have great wealth the UN is remiss to intervene. The good news is that being banned for being gay isn't going to affect his future applications to travel to countries where that's not a crime.
Best answer: We already knew the Left is intensely hypocritical, so yes.
How do I apply for SSI for my son that had a stroke and is in hospital? I have no photo.?


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All of a sudden, everyone's making a spectacle of themselves
People used to wear glasses just so they could see. Now, everyone from Michael Gove to Heston Blumenthal seems to wear them to make a statement
By Wendy Holden 15 October 2012 • 8:11pm
Visionary: the chef Heston Blumenthal has designed his own range of eyewear Credit: Photo: Rex Features
What do your glasses say about you? For many years it was just that you were short-sighted and, if you wore National Health ones, poor as well. There were very few variations. If your specs were jewelled and flicked up at the ends, you were Edna Everage; if they had blue lenses and stars around the edges, you were Elton John.
Then came the widespread use of contact lenses, of course, after which designers began to realise that people would need to look good in glasses if they were ever to put them on again. Now specs are everywhere once more, and not merely flattering, but meaningful. Loaded with symbolism. Infinite in their subtlety. Political, even.
Michael Gove, the Education Secretary, last week unveiled a smart new pair of bins along with a new anti-Europe push to the Right. Gove's barely visible rimless lenses of recent years have been dumped for a pair as emphatic, old-school and out-there as his new political position. They're not exactly flattering – early BBC presenters wore glasses like these, and Reginald Maudling, and people at Rotary Club dinners in the Fifties. But it's possible that vanity is less the issue here than the spectacles' suggestion of a more certain age, an age of overcoats and grammar schools and Great British Values. The synchronicity of Gove's new "Reginald Maudlings" with his anti-Brussels stance was striking, sending out the message that while a clear view is important, you've got to be doing it through the right frames. Is this what political "focus groups" have been thinking about all along?
Toby Young, take note. The writer and scourge of the state school system is reportedly considering throwing his hat into the ring as a Tory candidate. But it's his glasses that he really needs to think about. Toby's bins of the moment make him look much too much like Heston Blumenthal (of whom more later) and not enough like a serious legislator. A pair of owlish "Mr Chips" frames, hinting at back-to-basics education, would be a more appropriate advertisement of his free-schools-establishing politics. But no matter what style they are, to see a leading politician permanently in glasses would be a sight for sore eyes. It is striking how few prominent MPs wear specs. And it seems unlikely that they all have perfect sight. Is it vanity? Or do they fear that a visual admission of visual issues would make us all suspect that they were short-sighted in other ways, too? Or perhaps they fear to enter the lists, knowing how complicated, binswise, things are these days. The literally spectacular explosion of choice has blown all the old rules out of the water. Take cleverness. Glasses have historically signified brains, but until recently only in a slightly risible, University Challenge-geek sort of way. Enter TV's A History of Britain and Simon Schama's "Teutonic lozenges" and now that same sleek rectangular design casts a hip-sexy-academic air over the activities of everyone from Fabio Capello to Nigel Slater by way of Antony Gormley.
Famous people, especially those in lower brow professions – Madonna, Katie Price, Marilyn Monroe – have long worn glasses in the hope that someone might take them seriously. This, however, is no longer enough. You now need to specify which sort of seriously you'd like to be taken. Arty, tinted and round like Johnny Depp? Or heavy and fashiony like Gok Wan and Brad Pitt? Some hyper-celebrities signify their blazing proximity to the scorching sun of fame by wearing glasses like welder's goggles – I'm thinking of Bono, of Heston Blumenthal again. These are not glasses for civilians. Well I say that, but Heston's just designed his own range of specs for Vision Express, which will be available to all in the spring.
But are all of these people barking up the wrong tree? Some of the most iconic spectacle-wearers of the past, after all, wore glasses that people wouldn't be seen dead in now and yet managed to be geniuses, babe magnets and immortally respected. Take Stravinsky: short, spectacularly thick-lensed and yet the lover of Coco Chanel as well as the coolest man in Paris following the Rite of Spring. Ditto Prokofiev and Shostakovich, not to mention Groucho Marx.
Perhaps this is why one category of specs-wearer rises above the melee and takes the line they have for generations. The Queen, year after year, turns down the wattage of a glittering crown with a pair of enormous pensioner-style bifocals. Can she see something the others can't?
Wendy Holden's new novel, 'Gifted and Talented', is out in 2013
MI5's intervention on China marks a watershed moment
Julia Pamilih 17 Jan 2022, 3:13pm


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Wolff makes Aston Martin investment, committed to Mercedes F1 role
Jonathan Noble
18 April 2020, 4:39 am ·2-min read
Wolff makes personal Aston Martin investment
Mercedes Formula 1 boss Toto Wolff has made a personal investment in Aston Martin, Autosport has learned, but he remains fully committed to his current role at the title-winning team.
As recently reported, Wolff has been considering a private purchase of Aston Martin shares in the wake of Lawrence Stroll's recent buy-in.
Stroll is a friend of Wolff's, and his Racing Point team has a close alliance with Mercedes as one of its customer teams.
While Wolff has repeatedly denied that he will take a formal role at the British sportscar manufacturer, amid speculation he could become CEO, buying shares as an investment has long been on the table.
While such an investment would seem unusual considering his role at Mercedes, the German car manufacturer's parent company Daimler is a long term shareholder in Aston Martin - so there is no conflict of interest.
Daimler struck a deal in 2013 to receive what was then 5% of shares (non-voting) in exchange for supplying its next generation of cars with high-performance engines and electronic components.
Daimler is now Aston Martin's largest supplier and, as confirmed in Aston Martin's latest prospectus last week, has had a veto over any future investment partners.
It is understood that Toto has purchased a 4.77% stake in Aston Martin which, following a rights issue that will dilute the investment, will be worth 0.95% of the company next week.
A spokesperson for Mercedes said: "Fully diluted following the pending rights issue, this investment will represent a 0.95% stake in the company.
"It is a financial investment and Toto's partnership and executive role with Mercedes are unaffected by the transaction."
Wolff is currently in discussions with Mercedes about extending his contract to remain at the German car manufacturer
While he could change the specifics of his role, it appears almost certain that he will remain on board for the near future.
Speaking to Austrian media recently, Wolff said: ""I'm in the eighth year now. I love sports and this team.
"However, I am somewhat surprised by the turn of events over the winter and by the behaviour of individual people.
"Of course, this also has to do with my decision on what to do in 2020 and beyond.
"But I am and will remain the head of Mercedes Motorsport and F1 boss, and nothing will change in the short term."
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Liverpool vs Manchester United: Visitors miss chance to erase suspicion of title credentials
Rivals drew at Anfield but there was a winner in the title race: Manchester City
Jurgen Klopp happy with Liverpool performance in Manchester United draw despite another goalless outing
The Reds missed the chance to regain top spot in the league
Everything you need to know ahead of the match
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Liverpool 0-0 Manchester United LIVE! Premier League result, match stream, news and Solskjaer, Klopp reaction
Goalkeeper Alisson Becker came to his side's rescue to preserve Liverpool's unbeaten home league record in a goalless draw at home to arch-rivals Manchester United. The top-of-the-table clash between England's two most decorated clubs never got close to fulfilling its billing, with the best quality on show being that from the Liverpool keeper, who twice denied Bruno Fernandes in the second half. Manager Jurgen Klopp's 200th Premier League match in charge - and his 100th at Anfield - will not live long in the memory, with a predictable seventh draw in the last 10 meetings between these sides.
Liverpool 0-0 Manchester United: Man Utd stay top of the table as Allison saves Premier League champions
Manchester United remain three points clear of Liverpool at the top of the Premier League table after the two sides shared a goalless draw at Anfield on Sunday. Allison Becker made two big saves from Bruno Fernandes and Paul Pogba as United went for the win late on, but a draw was a fair result on the balance of play on Merseyside. United sat back and looked to counter in a cagey first half with little in the way of chances for either side.
The Reds goalkeeper twice denied midfielder Bruno Fernandes.
Tanguy Ndombele goal: Jose Mourinho hails Tottenham star's 'genius' for wonder strike vs Sheffield United
Jose Mourinho described Tanguy Ndombele's wonder-goal against Sheffield United as "genius" but said he cared more about the midfielder's overall performance in the 3-1 win at Bramall Lane. Ndombele scored an outrageous lob to restore the visitors' two-goal advantage, moments after David McGoldrick halved the deficit on the hour. Serge Aurier gave Spurs the lead after five minutes, with Ndombele also involved in the build-up, and Harry Kane made it two before the interval, as Mourinho's men returned to winning ways in the Premier League.


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Fast Company Chronicles the Changing Face of Business
Inside Flipboard / November 18, 2011
A business publication for the 21st century, Fast Company was founded in 1995 by Alan Webber and Bill Taylor, two former Harvard Business Review editors. The magazine was born at the dawn of a (still-ongoing) revolution, with a mission to chronicle the companies reinventing business through innovations in technology, business models, and management. This was not your father's fusty, old trade publication: its use of photography and design forever changed the way that business magazines looked.
Today, Fast Company is more relevant than ever—especially because starting now, it's customized for Flipboard. The people and companies inventing the future come to life in the magazine's smart articles about startups, leadership, ethonomics (ethical economics), trends, branding, social media, and design.
Fast Company's beautiful Flipboard edition also includes articles from sister publications Co.Design, devoted to the intersection of business and design, and the new Co.Exist, a daily tour of the latest ideas in transportation, energy, education, food, and health.
You can read Fast Company on Flipboard by tapping the button below, and if you like what you see, tap the blue "Add" button to make it an essential part of your everyday reading experience.
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O'Hara upperclass receive class rings
wnycatholic December 10, 2021
Among the students and parents who attended the Cardinal O'Hara High School class ring ceremony are (from left,) Michael and Brandy Lakeman and their daughter Marissa, a senior, and Rachel and Leonard Smith with their ...
Seniors get a treat from O'Hara students
wnycatholic November 3, 2021
Costumed students from Cardinal O'Hara High School made their annual trick or treat visit to seniors living at Crestmount Senior Apartments in the Town of Tonawanda on Friday, Oct. 29. Students and residents enjoyed the Halloween ...
O'Hara senior makes mark in alternate music world
wnycatholic October 26, 2021
TONAWANDA — Determined, committed, unwavering, persevering, a self-starter and go-getter are but a few words that describe Emily Lyman, a senior at Cardinal O'Hara High School. As early as age 12, Emily followed alternative rock, ...
Education, Uncategorized
O'Hara Hall of Fame honors alumni
wnycatholic October 8, 2021
Members of the'89 baseball team that won 2 post season championships, the Georgetown Cup and the Mayor's Trophy, joined for some reminiscing and fun. Team members include, (standing from left) Chris Sidote, Frank Montaldi, Mike ...
O'Hara congratulates sports champs with Athletic Hall of Fame inductions
TONAWANDA — Cardinal O'Hara High School will honor new inductees into the school's Athletic Hall of Fame on Oct. 2, at 5:30 p.m., at Banchetti by Rizzo's in Amherst. Inductees include individuals and teams that ...
Cardinal O'Hara inducts 9 into Hall of Fame
TONAWANDA — Cardinal O'Hara High School will honor new inductees into the school's Hall of Fame at a banquet and ceremony on Oct. 2, at 5:30 p.m., at Banchetti by Rizzo's in Amherst. Candidates, selected ...
Bishop Fisher, Education
Bishop and superintendent tour Cardinal O'Hara campus
Patrick J. Buechi September 9, 2021
Bishop Michael W. Fisher learns about the recently renovated chapel at Cardinal O'Hara High School from Principal Mary Holzerland. The bishop visited the Tonawanda institute on the first day of school. (Photo by Patrick J. ...
Cardinal O'Hara cheers for gold medal winner
USA's Sydney Mclaughlin celebrates with the national flag after arriving second the Women's 400m Hurdles final at the 2019 IAAF Athletics World Championships at the Khalifa International stadium in Doha on Oct. 4, 2019. Photo ...
Hawks return with a great gift
Patrick J. Buechi August 2, 2021
Five founding members of the COHS Thanks-A-Million Campaign gather to celebrate their 50 year reunions at the O'Hara Fest which took place at the school July 30. From left, Paul '70 and Kathryn '71 Murray, ...
Cardinal O'Hara golf outing kicks off 60th year celebration
wnycatholic July 22, 2021
TONAWANDA — Cardinal O'Hara High School will sponsor its annual Alumni Golf Outing on Thursday, Aug. 26 at Rothland Golf Course in Akron. The outing is open to all alumni and friends and is one ...