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

Magnetars are ultra-highly magnetized neutron stars (inferred surface
dipolar field strengths $B_s \approx 10^{14-15}$\,G) that display
hugely variable and sometimes very bright X-ray emission, powered
by their decaying fields \citep{dt92a}.  This process is reflected
in their extremely unsteady rotation.  Their magnetic fields cause
magnetars to spin down very rapidly, and all those known have long
periods, $2<P<12$\,s.

Among the 23 known magnetars
\citep{ok14}\footnote{\url{http://www.physics.mcgill.ca/~pulsar/magnetar/main.html}.},
four are known to be transient emitters of radio pulsations.  The
first to be so identified was the $P=5.54$\,s anomalous X-ray pulsar
(AXP) \xte, discovered in early 2003 following an X-ray outburst
\citep{ims+04}.  It is unclear when radio emission started, but
pulsations were not present in 1998, while a point source was visible
by early 2004 \citep{hgb+05}.  Radio pulsations were detected in
early 2006 \citep{crh+06}, with some properties that are markedly
different from those of ordinary rotation-powered pulsars, including
extremely variable flux densities and pulse profiles, and flat
spectra \citep[e.g.,][]{crp+07,ljk+08}.  The emission is also highly
linearly polarized, like that of several ordinary young radio pulsars
\citep{crj+07,ksj+07}.  To a great extent, these properties are
shared by all four radio magnetars identified so far
\citep{crhr07,crj+08,lbb+10,kjlb11,sj13}.

The radio emission from \xte\ arose following the X-ray outburst.
The X-ray flux then decayed exponentially and returned to pre-outburst
levels in 2007--2008 \citep{bpg+11}.  Here we show that \xte\ ceased
to emit detectable radio pulsations in late 2008, and present the
timing, flux density, polarimetric, and pulse profile behavior
during its last 20 months of radio activity.  We also present X-ray
timing measurements and fluxes through 2014.

\section{Radio Observations}\label{sec:obs}

Our previously published radio studies of \xte\ (also known as
PSR~J1809$-$1943) are based on extensive data sets largely from
2006.  Here we present results based on observations done with the
Robert C.\ Byrd Green Bank Telescope (GBT), the Nan\c{c}ay
radio telescope (NRT), and the CSIRO Parkes telescope, mainly
through the end of 2008.  Table~\ref{tab:sens} summarizes
relevant parameters for all the radio observations presented in
this paper.

\begin{deluxetable}{lllll}
\tabletypesize{\footnotesize}
\tablewidth{0pt}
\tablecolumns{5}
\tablecaption{\label{tab:sens}Parameters and Sensitivities for Radio Observations of \xte}
\tablehead{
\colhead{}  & \colhead{NRT} & \colhead{PKS AFB} &
\colhead{PKS DFB} & \colhead{GBT} }
\startdata
Center frequency (MHz) & 1398   & 1374              & 1369     & 1950   \\
Bandwidth (MHz)        &   64   &  288              &  256     &  600   \\
Gain, $G$ (K\,Jy$^{-1}$) & 1.55\tablenotemark{a} & 0.735\tablenotemark{b} & 0.735\tablenotemark{b} & 1.9\tablenotemark{c} \\
System temperature, $T_{\rm sys}$ (K) & 47\tablenotemark{d} & 44 & 44 & 28 \\
SEFD\tablenotemark{e} (Jy) & 30\tablenotemark{f} & 60\tablenotemark{g} & 60\tablenotemark{g} & 15\tablenotemark{h} \\
$\eta$ & 1.0 & $\sqrt{(\pi/2)}$\tablenotemark{i} & 1.0 & 1.2\tablenotemark{j} \\
SEFD$_{\rm eff}$\tablenotemark{k} (Jy) & 30 & 76 & 60 & 17
\enddata
\tablecomments{Observations used the
Berkeley-Orl\'eans-Nan\c{c}ay (BON) coherent dedispersor \citep{ct06} at the
NRT,
the analog \citep[AFB;][]{mlc+01} and digital
\citep[DFB;][]{mhb+13} filterbanks at Parkes, and the pulsar
Spigot \citep{kel+05} at the GBT. Sensitivity parameters are given in the
direction of \xte\ for the specified frequencies and bandwidths.
The sky temperature at 1.4\,GHz in this direction is $T_{\rm sky}
= 16.4$\,K including CMB (obtained from
\url{http://www3.mpifr-bonn.mpg.de/survey.html}; \citealt{rtr01}).}
\tablenotetext{a}{\citet{tch+05}.}
\tablenotetext{b}{Nominal $G$ of multibeam receiver center pixel
\citep{mlc+01}.}
\tablenotetext{c}{\url{http://www.gb.nrao.edu/~fghigo/gbtdoc/sens.html}.}
\tablenotetext{d}{$T_{\rm sky}$ plus ``no-sky'' $T_{\rm
sys} = 30$\,K (given cold-sky $T_{\rm sys} = 35\,$K;\\ \url{http://www.nrt.obspm.fr/nrt/obs/NRT_tech_info.html}).}
\tablenotetext{e}{System equivalent flux density ($\equiv T_{\rm sys}/G$).}
\tablenotetext{f}{Computed from $T_{\rm sys}$ and known $G$.}
\tablenotetext{g}{Calibrated assuming Hydra~A flux density of
42.5\,Jy at 1.4\,GHz \citep[after accounting for a 1.5\% beam
dilution factor;][]{bgpw77}.}
\tablenotetext{h}{Measured within Spigot band from flux-calibrated
GUPPI observation\\
(\url{https://safe.nrao.edu/wiki/bin/view/CICADA/GUPPiUsersGuide}).}
\tablenotetext{i}{Inefficiency factor due to AFB 1-bit sampling \citep{mlc+01}.}
\tablenotetext{j}{Estimated inefficiency factor due to Spigot 3-level
quantization \citep[cf.][]{kel+05}.}
\tablenotetext{k}{Effective SEFD ($\equiv \eta \times \mbox{SEFD}$),
used to compute \xte\ flux densities (see Sections~\ref{sec:flux}
and \ref{sec:spect}).}
\end{deluxetable}

\subsection{Radio Timing}\label{sec:timing}

In \citet{ccr+07} we showed the timing behavior of \xte\ through
2007 January, based largely on 1.4\,GHz data collected
with the BON spectrometer at the NRT.  As the flux density
decreased it became preferable to time the pulsar at the GBT.
We did this at 2\,GHz using the Spigot spectrometer,
recording the data in search mode and folding offline.
Nevertheless, BON timing continued to be important, particularly
during 2007 May--August when the GBT was not available. The
NRT observations were coherently dedispersed, with the full band
divided into 16 frequency channels, then folded at the predicted
pulsar period with 2 minute sub-integrations before mid-2007 and
30\,s thereafter. See Table~\ref{tab:toas} for a log of the timing
observations newly presented here.  Daily observations typically
lasted 1\,hr at Nan\c{c}ay and varied greatly at the GBT, from
0.25\,hr to 2\,hr with most at least 0.5\,hr (i.e., from a couple
of hundred to over 1000 pulsar rotations per session).

\begin{deluxetable}{lcc}
\tabletypesize{}
\tablewidth{0pt}
\tablecolumns{3}
\tablecaption{\label{tab:toas} Log of Radio Timing Observations of \xte}
\tablehead{
\colhead{MJD range (days)}  & \colhead{Number of daily TOAs} &
\colhead{Telescope} }
\startdata
54128--54218 (90)  & $53+18$ & $\mbox{GBT}+\mbox{Nan\c{c}ay}$ \\
54226--54357 (131) & 27    & Nan\c{c}ay                       \\
54352--54739 (387) & 51    & GBT
\enddata
\tablecomments{GBT TOAs were obtained with Spigot at 2\,GHz;
Nan\c{c}ay TOAs were obtained with BON at 1.4\,GHz (see
Section~\ref{sec:timing}). The average observing cadence in the
three periods listed decreased from once every 1.5 days, to once
every 5 days, to once every 7.5 days. }
\end{deluxetable}

In principle there are unusual challenges involved in radio timing
of \xte, because of changing pulse profiles.  In practice we found
that on the vast majority of days a simple procedure was sufficient
to obtain times-of-arrival (TOAs) that could be used to describe
reliably the rotation of the star.  We first excised strong
radio frequency interference from the BON and Spigot data. BON
timing was detailed in \citet{ccr+07}.  For Spigot we obtained TOAs
by cross-correlating individual folded pulse profiles with a Gaussian
template.  We then used the TOAs with the TEMPO
software\footnote{\url{http://tempo.sourceforge.net}.} to obtain
timing solutions.

\begin{figure}
\begin{center}
\includegraphics[angle=0,scale=0.42]{fig1.eps}
\caption{\label{fig:fdotflux}
Torque and radio flux density of \xte.  (a) Frequency derivative
versus date (Section~\ref{sec:timing}).  Measurements from
before MJD~54127 (2007.1) are reproduced from \citet{ccr+07}. (b)
Period-averaged flux density versus date.  Data from before
2007.1 were presented in \citet{ccr+07} but have been reanalyzed
for this paper (see Section~\ref{sec:flux}).  }
\end{center}
\end{figure}

The position of \xte\ was held fixed in all our timing fits at that
determined from VLBI observations \citep{hcb+07}; the measured
proper motion is too small to affect the timing of this pulsar.  As
explained in \citet{ccr+07}, we maintained phase connection for
this pulsar since 2006 April, but the rotation frequency derivative
was changing so rapidly that it proved more informative to measure
$\dot \nu$ (where $\nu = 1/P$) by using TOAs typically spanning one
month and doing a TEMPO fit for only $\nu$ and $\dot \nu$.  We did
such fits in segments of data offset by roughly 15 days to provide
good sampling of $\dot \nu$, and the results are shown in
Figure~\ref{fig:fdotflux}a.  In this panel, the first 17 measurements
are reproduced from \citet{ccr+07}, while the next 33 measurements
are new.

\begin{figure}
\begin{center}
\includegraphics[angle=0,scale=0.42]{fig2.eps}
\caption{\label{fig:timing}
Timing residuals for \xte.  (a) Phase residuals versus date for a
timing model that fits only for rotation phase, frequency, and
frequency derivative, showing a cubic trend.  (b) Residuals for a
model that fits for phase, $\nu$, $\dot \nu$, and $\ddot \nu$ (see
Section~\ref{sec:timing} and Table~\ref{tab:parms}).  }
\end{center}
\end{figure}

\begin{deluxetable}{ll}
\tabletypesize{}
\tablewidth{0pt}
\tablecolumns{2}
\tablecaption{\label{tab:parms} Two Radio Timing Solutions for \xte}
\tablehead{
\colhead{Parameter}  & \colhead{Value} }
\startdata
R.A. (J2000.0)                              & $18^{\rm h}09^{\rm m}51\fs087$  \\
Decl. (J2000.0)                             & $-19\arcdeg43\arcmin51\farcs93$ \\
Dispersion measure, DM                      & 178.0\,pc\,cm$^{-3}$            \\
Epoch (MJD TDB)                             & 54550.0                         \\
Range of dates (MJD)                        & 54352--54729                    \\
Frequency, $\nu$~\tablenotemark{a}          & 0.18048830377(8)\,Hz            \\
Frequency derivative, $\dot\nu$~\tablenotemark{a} & $-9.163(1)\times10^{-14}$\,Hz\,s$^{-1}$ \\
\tableline
Frequency, $\nu$~\tablenotemark{b}          & 0.1804882977(1)\,Hz    \\
Frequency derivative, $\dot\nu$~\tablenotemark{b} & $-9.090(2)\times10^{-14}$\,Hz\,s$^{-1}$ \\
Frequency second derivative, $\ddot\nu$~\tablenotemark{b} & $2.46(5)\times10^{-22}$\,Hz\,s$^{-2}$ \\
RMS post-fit timing residual ($P$)          & 0.007
\enddata
\tablecomments{The celestial coordinates were held fixed at the
values obtained from VLBA observations \citep{hcb+07}, and the DM
was held fixed at the value obtained from simultaneous 0.7 and
2.9\,GHz observations \citep{crh+06}. }
\tablenotetext{a}{These two parameters are sufficient to obtain a
phase-connected solution encompassing the MJD range, but do not
fully describe the rotation of the neutron star.  See
Figure~\ref{fig:timing}a and Section~\ref{sec:timing}. }
\tablenotetext{b}{These three parameters fully describe the rotation
of the neutron star within the given MJD range, but have little
predictive value outside it.  See Figure~\ref{fig:timing}b and
Section~\ref{sec:timing}. }
\end{deluxetable}

It is clear from Figure~\ref{fig:fdotflux}a that over the last $\sim
400$ days $\dot \nu$ stabilized greatly, compared to earlier
large variations.  To investigate this in detail we obtained
phase-connected fits spanning the last year of timing data.  In
Figure~\ref{fig:timing}a we show the residuals from a simple fit
to rotation phase, $\nu$, and $\dot \nu$, showing large residuals.
In Figure~\ref{fig:timing}b, we see that the addition of $\ddot
\nu$ absorbs all remaining residual trends.  These timing solutions
are listed in Table~\ref{tab:parms}.  The positive value of $\ddot
\nu$ implies that during this span $-\dot \nu$ (proportional to the
braking torque) was decreasing steadily, by a total of 9\% during
the year.

\subsection{Radio Flux Densities}\label{sec:flux}

One unusual aspect of radio emission from \xte\ is the fluctuation
on $\sim$ daily timescales of its period-averaged flux density,
largely intrinsic to the pulsar \citep[e.g.,][]{ljk+08}.  These
variations result from a combination of different pulse profile
components becoming active (i.e., because of radically changing
profiles) and varying intensity from particular components.
Superimposed on this apparently chaotic variation, the average flux
density of the pulsar decreased by over an order of magnitude in
the 10 months following its pulsed radio discovery, as
seen in Figure~\ref{fig:fdotflux}b (these pre-2007 data
were originally presented in \citealt{ccr+07} but have been reanalyzed
here in order to present a consistent flux density record).

Most period-averaged flux densities presented in this paper
(including all in Figure~\ref{fig:fdotflux}b) were obtained by
measuring for each daily observation the area under the pulse
profile, scaled to its off-pulse rms, and converting to a Jansky
scale using the observing parameters and telescope system
noise (cf.\ the SEFD$_{\rm eff}$ values in
Table~\ref{tab:sens}; see section 7.3.2 of \citealt{lk04} for more
details on this method).  We estimate that the absolute 1.4\,GHz
flux density scale is accurate to within 10\%.

The greatest source of uncertainty arises from the impact of radio
frequency interference (RFI) and system noise fluctuations on this
long period and, from 2007, faint pulsar.  Each pulse
profile was carefully excised of RFI in both the frequency and time
domains. Nevertheless, for approximately one-third of all
the post-2006 NRT observations, the RFI was so bad or the flux
density was so low (approaching the $\approx 0.1$\,mJy detection
threshold), that we did not extract a flux density measurement at
all. In some of the remaining instances, as much as half of the
data had to be discarded in order to obtain an integrated profile
clean enough to measure flux density. Mindful of these caveats (most
often some residual RFI is bound to remain, and individual measurements
could be greatly affected), we estimate that the NRT flux density
measurements in Figure~\ref{fig:fdotflux}b have a typical relative
fractional uncertainty of $\approx 20$\%, with a minimum of 0.1\,mJy.

Two things immediately stand out from Figure~\ref{fig:fdotflux}b:
daily flux density variations continued through the end of our data
set, by factors of a few; and the average 1.4\,GHz flux
density stabilized early in 2007, at a level of $0.68\pm0.27$\,mJy
for all post-2006 NRT detections presented here.  Also, the panels
of Figure~\ref{fig:fdotflux} are curiously something of a mirror
image to each other.

\subsubsection{Radio Disappearance}\label{sec:dis}

\begin{figure}
\begin{center}
\includegraphics[scale=0.90]{fig3.eps}
\caption{\label{fig:lastGBT}
Last radio detection of \xte\ at the GBT. The period-averaged flux
density is among the smallest we observed ($\sim 50\,\mu$Jy),
but pulse detection is aided by the ``spiky'' nature of its narrow
sub-pulses.  Two rotations are shown as a function of time, with
the summed profile at the top. White areas are subintegrations
masked due to particularly bad RFI.  }
\end{center}
\end{figure}

\begin{figure}
\begin{center}
\includegraphics[angle=0,scale=0.42]{fig4.eps}
\caption{\label{fig:nd}
Fourty-seven radio non-detections of \xte\ since late 2008
(Section~\ref{sec:dis}).  The dots represent measured
NRT flux densities, reproduced from Figure~\ref{fig:fdotflux}b.
The other symbols denote individual observations without a
detection, placed at approximately the upper flux density limits
for the respective sets of observations. }
\end{center}
\end{figure}

With no warning from either its timing or flux density behavior,
\xte\ ceased to emit detectable radio pulsations in late 2008.  The
last detection at the NRT was on October 29, on November
2 at the GBT (Figure~\ref{fig:lastGBT}), and at Parkes on the
following day.  The next attempt to detect it was on November 10.
We attempted to detect the pulsar at Parkes on 20 occasions
through 2016 January, largely at 1.4\,GHz, each time for 0.5--1\,hr.
At the NRT we did 10 more observations through 2009 June.
At the GBT we made a total of 17 attempts at 2\,GHz, each $\approx
0.5$\,hr, through 2012 August.  The pulsar was not detected in any
of these 47 observations spanning 7 years since
2008 November (Figure~\ref{fig:nd}).  We emphasize that \xte\ did
not gradually fade into undetectability.  A few weeks before the
last detection, we recorded beautiful profiles (e.g.,
Figures~\ref{fig:pol}d, \ref{fig:profs}c and \ref{fig:profs}d); the
signal strength and pulse profiles were fluctuating at least as
much as they had for the previous $\sim 500$ days.  And then the
radio pulses were gone.

For an assumed pulse duty cycle of 6\% (comparable to the
component widths often observed for this pulsar) and the parameters
used in our monitoring observations (Table~\ref{tab:sens}), the
upper limit on the flux density of \xte\ since late 2008 is
approximately 0.1\,mJy at 1.4\,GHz based on the NRT observations,
slightly lower than that for the Parkes observations, and approximately
0.03\,mJy at 2\,GHz based on the GBT observations (Figure~\ref{fig:nd}).
These limits are nearly an order of magnitude below the {\em
average\/} flux densities during the 1.8 years of radio emission
post-2006, although not much below the faintest established detections
(see Figures~\ref{fig:lastGBT} and \ref{fig:alpha}).  The great
profile variability, long period, and RFI, make more detailed
estimates unreliable. In any case, since the last detection in
late 2008, in none of 47 observations spanning 7
years was the pulsar as detectable as in the poorest of more than
200 detections made over a period of 2 years
before 2008 November.

\begin{figure}
\begin{center}
\includegraphics[angle=0,scale=0.42]{fig5.eps}
\caption{\label{fig:alpha}
Flux density measurements for \xte\ at 1.4\,GHz and 2\,GHz
in 2007--2008.  Parkes observations include those done with analog
(AFB) and full-Stokes digital (DFB) filterbanks.  See
Section~\ref{sec:spect} for details. }
\end{center}
\end{figure}

\begin{figure}
\begin{center}
\includegraphics[angle=0,scale=1.06]{fig6.eps}
\caption{\label{fig:pol}
Polarimetric pulse profiles of \xte\ recorded at Parkes.  Only 50\%
of pulse phase is shown. In each lower panel the black trace
represents total intensity, red is linear polarization, and blue
is circular.  Each upper panel shows the position angle of linear
polarization, rotated to the pulsar frame using
$\mbox{RM}=78$\,rad\,m$^{-2}$.  The profiles are phase-aligned with
respect to each other by eye, and absolute phase is arbitrary.
Recurring profile features are labelled P1--P5 (as in
Figure~\ref{fig:profs}). }
\end{center}
\end{figure}

\subsection{Radio Spectrum}\label{sec:spect}

The available evidence suggests that during the faint epoch
that lasted for 2 years preceding its radio disappearance in late
2008, \xte\ had a steep radio spectrum, contrasting to its earlier
generally flat spectrum.

In Figure~\ref{fig:alpha} we present all our post-2006 flux
density measurements at 1.4\,GHz and 2\,GHz. The 1.4\,GHz NRT values
are reproduced from Figure~\ref{fig:fdotflux}b. These are fundamentally
consistent with Parkes measurements at the same frequency from six
full-Stokes observations using pulsar digital filterbanks (DFBs),
analyzed with PSRCHIVE \citep{hvm04}, and 12 analog filterbank (AFB)
observations.

The 2\,GHz flux density values presented here were obtained
from a subset of the GBT data used to derive TOAs
(Section~\ref{sec:timing}), using the method outlined in
Section~\ref{sec:flux} for NRT and Parkes AFB observations.  We
determined the system noise (Table~\ref{tab:sens}) from a full-Stokes
2\,GHz observation in the direction of \xte, flux-calibrated with
PSRCHIVE.  Even after careful RFI excision, we selected for reliable
flux density measurements only 40\% of all observations from which
we extracted a TOA.  We estimate relative fractional uncertainties
of $\approx 20$\% on average.

The 2\,GHz measurements in Figure~\ref{fig:alpha} range
over 0.1--0.5\,mJy, with an average and standard deviation of $S_2
= 0.25\pm0.10$\,mJy.  This is to be compared to $S_{1.4} =
0.68\pm0.27$\,mJy for the 1.4\,GHz measurements in the figure
(Section~\ref{sec:flux}), spanning much the same time interval. At
face value this would seem to suggest a spectral index of $\alpha
\approx -3$ (where $S_\nu \propto \nu^{\alpha}$).  Given the inherent
difficulties in extracting such a measurement for this variable
pulsar from non-simultaneous multi-frequency observations susceptible
to RFI despite our best efforts, we do not claim a reliable numerical
value for $\alpha$.  But Figure~\ref{fig:alpha} strongly suggests
that \xte\ indeed became a steep-spectrum object during its final
``weak'' state prior to disappearance as a radio source, in that
respect more akin to an ordinary pulsar than earlier in its ``high''
state, when the torque was also varying rapidly
(Figure~\ref{fig:fdotflux}).

\subsection{Polarimetry}\label{sec:pol}

All of our previously published \xte\ polarimetric data are from
before 2006 December \citep{crj+07}.  The data published by
\citet{ksj+07} end even earlier, but include single-pulse polarimetry.
Here we present some polarimetric observations done in 2007 and
2008 with Parkes at 1.4\,GHz and 3\,GHz, using respectively the
center beam of the multibeam receiver and the 10\,cm band of the
1050cm receiver.  The data were collected using DFBs, and
analyzed with PSRCHIVE, as in \citet{crj+07}.

Figure~\ref{fig:pol}a is a reprocessed version of a 2006 observation
presented in \citet{crj+07}, differing mainly in the flux
density scale and amount of data excised due to RFI.  The recalculated
rotation measure is $\mbox{RM} = 76\pm1$\,rad\,m$^{-2}$, entirely
consistent with the value in \citet{crj+07}, and the RMs calculated
for the latter observations are consistent with this value within
their larger uncertainties.

The 3\,GHz full-Stokes profile (Figure~\ref{fig:pol}c) looks similar
to its counterpart from 1.5 years before \citep[Figure~1c of][]{crj+07}.
At 1.4\,GHz, the two 2007/2008 profiles (Figure~\ref{fig:pol}b and
\ref{fig:pol}d) show very similar position angles of linear
polarization (PA), and differ mainly in the relative amplitudes of
three total-intensity profile components (labelled P2, P3, and
P4/5). Both profiles are close to 100\% linearly polarized.

Comparison between the 2006 profile (Figure~\ref{fig:pol}a) and the
2007/2008 1.4\,GHz profiles shows that the PA sweep and its absolute
values are similar for the ``main pulse'' regions (components
P3--P5).  However, the 2007/2008 profiles show component P2 not
present in the 2006 profile --- whose P1 component in turn is not
seen later on.  Profile components P1--P5 altogether span 40\% of
pulse phase, and if they all display stable PAs between 2006 and
2007/2008, then in principle this allows for a more conclusive
investigation of geometry than previously possible (see
Section~\ref{sec:rvm}).

\subsection{Radio Pulse Profiles}\label{sec:profs}

\begin{figure}
\begin{center}
\includegraphics[angle=0,scale=1.21]{fig7.eps}
\caption{\footnotesize \label{fig:profs}
A selection of \xte\ radio pulse profiles. Prominent features in
the profile that reoccur are labelled P1--P5 (as in Figure~\ref{fig:pol}).
We define the ``main pulse'' (MP) region as being composed of up
to features P3--P5.  Profiles are aligned by eye, and the absolute
phase here is arbitrary.  }
\end{center}
\end{figure}

The total-intensity pulse profiles of \xte\ were always extremely
variable, both in phase of active emitting regions and in the daily
appearance of each pulse profile component.  The description that
follows is based on a review of hundreds of daily profiles that we
obtained during 2006--2008 at the GBT, Parkes, and Nan\c{c}ay.
There was never any stable pulse profile, but we detected emission
from some pulse longitudes more often than from others, with some
discernible patterns over time, and radio pulsations were never
detected from many longitudes.  In that sense, there was some
long-lasting stability to the radio-emitting region.

Referring to Figure~\ref{fig:profs}a, emission was always detected
from the main pulse region (MP, in turn made up of at least three
discernible sub-structures, labelled P3--P5, not all necessarily
emitting at once). Emission from component P1 (see also
Figure~\ref{fig:pol}a) was detected only during 2006, and it was
the most variable, sometimes being much brighter than the MP
components.  On the other hand, P2 was active sometimes in 2006 and
2007 (Figure~\ref{fig:pol}b), but became more common in 2008
(Figures~\ref{fig:pol}d and \ref{fig:profs}c--d).  In 2007 the
observed profile often consisted of emission from the MP region
alone (Figure~\ref{fig:profs}b). In only one (2006) observation out
of hundreds did we detect emission from all these regions at once
(Figure~\ref{fig:profs}a).

The relative amplitudes of the different components varied widely,
exemplified in Figure~\ref{fig:profs}d by P4, usually not preeminent
but on this day the brightest of any.  The very ``spiky'' nature
of the individual sub-pulses that built up the broader integrated
profile components \citep[see, e.g.,][]{ssw+09} continued to the
very end (Figure~\ref{fig:lastGBT}).

Our sense is that in 2007--2008 the profiles were less variable
than in 2006, but this impression may be biased by two factors: the
pulsar was much brighter in 2006, which allowed the detection of
very faint rarely observed components \citep[see Figure~2 of][]{ccr+07};
and the total integration (both in number and in average duration
of observations) was larger in 2006 compared to later.  In any case
it is clear that during the period when the torque had stabilized
by comparison to earlier huge variations, and when the period-averaged
flux density had also stabilized in an average sense at a low level
(Figure~\ref{fig:fdotflux}), the pulse profiles of \xte\ were still
varying at unprecedented levels compared to normal pulsars, and
continued to do so until radio pulsations disappeared.

\section{X-ray Observations}\label{sec:xray}

In order to search for clues to the disappearance of radio pulsations
from \xte, we reviewed all its archival \chandra\ and \xmm\ data
collected from 2003--2014.  Timing results from 2009 November onward
are newly published here.  Detailed spectroscopic and flux analysis
are presented in \citet{ah16}, with a summary of the fluxes
given in Section~\ref{sec:xrayflux}.  In summary, we find that the
X-ray fluxes stepped down to a minimum value around the time that
the radio pulsations shut off, and this is the only recognizable
event in X-rays that is plausibly contemporaneous with the disappearance
in radio.

\subsection{X-ray Timing}\label{sec:xraytiming}

\begin{deluxetable*}{lrlcrl}
\tabletypesize{\small}
\tablewidth{0pt}
\tablecolumns{6}
\tablecaption{Log of X-ray Timing Observations of \xte}
\tablehead{\colhead{Mission/Instrument} & \colhead{ObsID } & \colhead{Date} &
\colhead{Epoch} & \colhead{\hfill Exposure} & \colhead{Frequency} \\
& & \colhead{(UT)} & \colhead{(MJD)} & \colhead{(ks)} &  \colhead{(Hz)}}
\startdata
\chandra\ HRC    & 4454       & 2003 Aug 27 & 52878 &  2.8 & 0.180531(11)    \\
\xmm\ pn+MOS     & 0161360301 & 2003 Sep  8 & 52890 & 12.1 & 0.18052682(30)  \\
\xmm\ pn         & 0152833201 & 2003 Oct 12 & 52924 &  8.9 & 0.1805245(12)   \\
\chandra\ HRC    & 5240       & 2003 Nov  1 & 52944 &  2.8 & 0.180536(10)    \\
\xmm\ pn+MOS     & 0161360501 & 2004 Mar 11 & 53075 & 18.9 & 0.18052415(25)  \\
\xmm\ pn+MOS     & 0164560601 & 2004 Sep 18 & 53266 & 28.9 & 0.18051856(18)  \\
\xmm\ pn+MOS     & 0301270501 & 2005 Mar 18 & 53447 & 42.2 & 0.18051142(16)  \\
\xmm\ pn+MOS     & 0301270401 & 2005 Sep 20 & 53633 & 42.2 & 0.1805046(3)    \\
\xmm\ pn+MOS     & 0301270301 & 2006 Mar 12 & 53806 & 51.4 & 0.1804991(4)    \\
\chandra\ ACIS-S & 6660       & 2006 Sep 10 & 53988 & 30.1 & 0.1804942(14)   \\
\xmm\ pn+MOS     & 0406800601 & 2006 Sep 24 & 54002 & 50.3 & 0.18049355(34)  \\
\xmm\ pn+MOS     & 0406800701 & 2007 Mar  6 & 54165 & 68.3 & 0.18049117(27)  \\
\xmm\ pn+MOS     & 0504650201 & 2007 Sep 16 & 54359 & 74.9 & 0.18048987(19)  \\
\chandra\ ACIS-S & 7594       & 2008 Mar 18 & 54543 & 29.6 & 0.1804868(15)   \\
\xmm\ pn+MOS     & 0552800201 & 2009 Mar  5 & 54895 & 65.8 & 0.18048610(24)  \\
\xmm\ pn+MOS     & 0605990201 & 2009 Sep  5 & 55079 & 21.6 & 0.1804857(13)   \\
\xmm\ pn+MOS     & 0605990301 & 2009 Sep  7 & 55081 & 19.9 & 0.1804829(16)   \\
\xmm\ pn+MOS     & 0605990401 & 2009 Sep 23 & 55097 & 14.2 & 0.1804872(24)   \\
\chandra\ ACIS-S & 11102      & 2009 Nov  1 & 55136 & 25.1 & 0.1804852(16)   \\
\chandra\ ACIS-S & 12105      & 2010 Feb 15 & 55242 & 12.6 & 0.180476(6)     \\
\chandra\ ACIS-S & 11103      & 2010 Feb 17 & 55244 & 12.6 & 0.180484(6)     \\
\xmm\ pn+MOS     & 0605990501 & 2010 Apr  9 & 55295 &  9.9 & 0.1804820(48)   \\
\chandra\ ACIS-S & 12221      & 2010 Jun 07 & 55354 & 10.0 & 0.180489(8)     \\
\xmm\ pn+MOS     & 0605990601 & 2010 Sep  5 & 55444 & 11.3 & 0.1804771(40)   \\
\chandra\ ACIS-S & 13149      & 2010 Oct 25 & 55494 & 15.4 & 0.1804766(35)   \\
\chandra\ ACIS-S & 13217      & 2011 Feb  8 & 55600 & 15.0 & 0.1804835(35)   \\
\xmm\ pn+MOS     & 0671060101 & 2011 Apr  3 & 55654 & 22.9 & 0.1804796(13)   \\
\xmm\ pn+MOS     & 0671060201 & 2011 Sep  9 & 55813 & 15.9 & 0.1804751(18)   \\
\chandra\ ACIS-S & 13746      & 2012 Feb 19 & 55976 & 20.0 & 0.1804790(23)   \\
\chandra\ ACIS-S & 13747      & 2012 May 24 & 56071 & 20.0 & 0.1804774(21)   \\
\xmm\ pn+MOS     & 0691070301 & 2012 Sep  6 & 56176 & 17.9 & 0.1804721(17)   \\
\xmm\ pn+MOS     & 0691070401 & 2013 Mar  3 & 56354 & 17.9 & 0.1804722(18)   \\
\xmm\ pn+MOS     & 0720780201 & 2013 Sep  5 & 56540 & 24.5 & 0.1804721(12)   \\
\chandra\ ACIS-S & 15870      & 2014 Mar  1 & 56717 & 20.1 & 0.1804723(20)   \\
\xmm\ pn+MOS     & 0720780301 & 2014 Mar  4 & 56720 & 25.0 & 0.1804682(11)   \\
\chandra\ ACIS-S & 15871      & 2014 Sep  7 & 56911 & 20.1 & 0.1804710(23)
\enddata
\label{tab:xraylog}
\end{deluxetable*}

\begin{figure}
\begin{center}
\includegraphics[width=0.98\linewidth]{fig8a.eps}
\end{center}
\vspace{-0.1in}
\begin{center}
\includegraphics[width=0.98\linewidth]{fig8b.eps}
\end{center}
\vspace{-0.1in}
\begin{center}
\includegraphics[width=0.98\linewidth]{fig8c.eps}
\end{center}
\vspace{-0.1in}
\caption{\footnotesize \label{fig:xray}
X-ray timing and flux properties of \xte\ from \chandra\ and \xmm.
(a) Frequency measurements, where the points linked with
the solid line in 2009--2012 comprise the phase-connected solution
in Table~\ref{tab:xraytime}.  The dashed line segment is the radio
timing solution from Table~\ref{tab:parms}.  (b) Frequency
derivatives obtained by differencing adjacent frequency measurements,
and from the 2009--2012 phase-connected solution.  The vertical
lines denote the first two epochs of radio detection at 1.4\,GHz
with the VLA \citep{hgb+05,crh+06}, and the shaded region encompasses
the epochs of pulsed radio detection from Figure~\ref{fig:fdotflux}.
It is not known whether radio emission at the flux density level
of the first detection ($4.5\pm 0.5$\,mJy) was present earlier in
the X-ray outburst, which was detected in 2003 January.  (c)
X-ray flux measurements from the three- or two-temperature blackbody
fits of \citet{ah16}.  Open triangles are the sum of the varying
hot and warm areas, and filled squares are the total flux including
the triangles and the cooler full surface area of the neutron star
represented by the (constant) dashed line. }
\end{figure}

Table~\ref{tab:xraylog} is a log of all \xte\ timing observations
performed by \chandra\ and \xmm\ through 2014.  The \chandra\ ACIS
observations were taken with the source on the S3 CCD, and with a
subarray of 100 or 128 rows to obtain time resolution of 0.3\,s or
0.4\,s, respectively. \xmm\ observations used the pn CCD in full-frame
or large-window mode, with 74\,ms or 44\,ms resolution and, in most
cases, the MOS CCDs in small-window mode with 0.3\,s resolution.
We corrected the processed archival \xmm\ photons for leap seconds
and time jumps when needed, and applied the barycentric correction
at the VLBI measured position.  We then computed frequencies and
$1\,\sigma$ errors using the $Z_1^2$ test on photons in the 0.3--4\,keV
band.  The two short \chandra\ HRC observations that were obtained
for the purpose of source location have relatively uncertain
frequencies, and were not used in the subsequent analysis.

The frequency measurements are shown in Figure~\ref{fig:xray}a.
These were used to track the time-varying frequency derivative from
2003--2009 by computing the difference in frequency between adjacent
\xmm\ observations, usually 6 months apart. Where these
$\dot \nu$ measurements overlap with the more precise record obtained
from radio observations during 2006--2008 (Figure~\ref{fig:fdotflux}a),
they agree. Figure~\ref{fig:xray}b illustrates that $\dot \nu$
varied by a factor of $\approx 6$.  In the months immediately
following the outburst, which was first detected in 2003 January,
monitoring by {\em RXTE\/} showed noisy spin-down with an even
higher mean frequency derivative of $-6.7\times 10^{-13}$\,Hz\,s$^{-1}$
\citep{ims+04}, which is $\approx 8$ times the minimum value of
$\approx -8 \times 10^{-14}$\,Hz\,s$^{-1}$ measured by \xmm\ in
2007--2008 (Figure~\ref{fig:xray}b).

Starting in 2009 September, more frequent observations allowed a
phase-connected solution to be established up through 2012 May.
This process was facilitated by the relatively stable spin-down
with small rate at later times.  Beginning with the two observations
on 2009 September 5 and 7, we folded the photons jointly using the
$Z_1^2$ test, and used the resulting frequency to fold the next
observation, verifying that the predicted phase agrees with the
observed one to $<0.2$ cycles.  Each subsequent observation was
then added to the joint fit and the  $Z_1^2$ test was iterated with
free parameters $\nu$ and $\dot \nu$, and finally $\ddot \nu$, until
15 observations were included.  The resulting fit is shown by the
solid line in Figure~\ref{fig:xray}a, and its $\dot \nu = -9.21
\times 10^{-14}$\,Hz\,s$^{-1}$ (Table~\ref{tab:xraytime}) is very
nearly a continuation of the minimum spindown rate that was first
reached in 2007.  The second frequency derivative as listed in
Table~\ref{tab:xraytime} is necessary to fit the 2009--2012 series
with a continuous ephemeris.

\begin{deluxetable}{ll}
\tabletypesize{}
\tablewidth{0pt}
\tablecolumns{2}
\tablecaption{X-ray Timing Solution for \xte}
\tablehead{
\colhead{Parameter} & \colhead{Value}
}
\startdata
R.A. (J2000.0)                   & $18^{\rm h}09^{\rm m}51\fs087$             \\
Decl. (J2000.0)                  & $-19\arcdeg43\arcmin51\farcs93$            \\
Epoch (MJD TDB)                  & 55444.0                                    \\
Range of dates (MJD)             & 55079--56071                               \\
Frequency, $\nu$                 & 0.18048121539(63)\,Hz                      \\
Frequency derivative, $\dot \nu$ & $-9.2121(35) \times 10^{-14}$\,Hz\,s$^{-1}$\\
Frequency second derivative, $\ddot \nu$ & $4.1(3)\times10^{-23}$\,Hz\,s$^{-2}$ \\
Surface dipole magnetic field, $B_s$\tablenotemark{a} & $1.3\times 10^{14}$\,G\\
Spin-down luminosity, $\dot E$\tablenotemark{b}       & $6.6\times 10^{32}$\,erg\,s$^{-1}$ \\
Characteristic age, $\tau_c$\tablenotemark{c}         & 31\,kyr
\enddata
\tablenotetext{a}{$B_s = 3.2\times10^{19} (P\dot P)^{1/2}$\,G, with
$P$ in s, where $P=1/\nu$.}
\tablenotetext{b}{$\dot E = 4 \pi^2 \times 10^{45} \dot
P/P^3$\,erg\,s$^{-1}$.}
\tablenotetext{c}{$\tau_c = P/(2\dot P)$.}
\label{tab:xraytime}
\end{deluxetable}

Analyzing the same data from which we established the phase-connected
ephemeris of Table~\ref{tab:xraytime}, \citet{pbm+16} claimed to
identify a timing anomaly in which the pulsar was spinning up
(positive $\dot\nu$) between 2010 September and 2011 February.  This
could have arisen from their underestimation of uncertainties in
frequency measurements. In any case, our phase-coherent ephemeris
spanning this time shows no such event. \citet{pbm+16} also propose
that there is a single phase-connected timing solution spanning all
of 2007--2014. This is clearly invalid, because their listed
uncertainties on the polynomial coefficients ($\nu$, $\dot \nu$,
$\ddot \nu$) are two orders of magnitude larger than what would be
needed to describe a unique cycle count. Also, the parameters of
our actual phase-coherent timing segments in radio (Table~\ref{tab:parms})
and X-ray (Table~\ref{tab:xraytime}) disagree with theirs.  In
particular, their fitted $\dot\nu=-4.9\times10^{-14}$\,Hz\,s$^{-1}$
is about half of the true value.

After 2012 May we were unable to maintain phase connection.  The
prior coherent timing solution fails to predict the phase of the
2012 September observation by $\approx0.5$ cycles.  Possibly an
anti-glitch \citep{akn+13,sag14} and/or change in torque occurred
between 2012 May and September.  But we cannot tell for sure what
happened because the change in frequency differs from the extrapolation
by only $2\,\sigma$.  We can only estimate the frequency derivative
from 2012 September to 2014 September with an incoherent fit to the
frequencies, which is highly uncertain.  All we can say is that the
long-term frequency derivative did not clearly change in 2012 (see
Figure~\ref{fig:xray}b).

From 2009 September to 2012 May, $\dot \nu$ changed by at most 4\%,
as measured by the frequency second derivative (which is a factor
of 6 smaller than that measured over the year following 2007
September; Table~\ref{tab:parms}).  Such behavior is common in AXPs
and soft gamma repeaters (SGRs), which often show extended periods
of smooth spin-down at small $|\dot \nu|$ as well as noisier epochs
with larger $|\dot \nu|$
\citep{kcs99,kgc+01,gk02,wkg+02,wkf+07,tgd+08,dkg09,dk14}.  At one
time, it was proposed that the combined action of free and radiative
precession could explain ``bumpy'' spin-down of AXPs \citep{mel99,mel00},
which predicted that $\dot \nu$ would oscillate with a period of
several years.  However, as observations of dramatic changes in
$\dot \nu$ from magnetars have accumulated over the years, none are
apparently dominated by such periodic variations (see
references above). There is at best some evidence possibly
indicating quasi-periodic $\dot \nu$ behavior in one magnetar
\citep{akn+15}. The timing behavior of \xte\ shown in
Figure~\ref{fig:xray} seems typical when compared with other magnetars
that have been monitored for longer times with no cyclic pattern
evident in their spin-down.

Figure~\ref{fig:xraypulse} shows three sample energy-dependent X-ray
pulse profiles from \xmm, during (2007) and after (2009, 2011) the
epoch of pulsed radio detection. They share the same characteristics
as earlier observations, in particular those from 2005 and 2006 as
shown in \citet{gh07b}.  The pulse peaks are in phase as a function
of energy, while the pulsed fraction increases sharply with energy.
This is understood in a model in which a small hot spot is surrounded
by a cooler, larger annulus that covers most of the neutron star.
In summary, there is no obvious change in X-ray timing or pulse
shapes corresponding to the shut-down of radio emission in late
2008.

\begin{figure*}
\begin{center}
\includegraphics[width=0.90\linewidth]{fig9.eps}
\end{center}
\caption{\label{fig:xraypulse}
Energy-dependent pulse profiles of \xte\ from three \xmm\ observations.
Background has been subtracted, and the counts per bin are normalized
so that the average is 1 in each panel. The profiles are centered
on phase 1, which is arbitrary with respect to the radio phases as
displayed in Figures~\ref{fig:pol} and \ref{fig:profs}. }
\end{figure*}

\subsection{X-ray Fluxes}\label{sec:xrayflux}

Figure~\ref{fig:xray}c summarizes the results from blackbody spectral
modelling that is described in more detail in \citet{ah16}.  The
spectrum is fitted with either two or three blackbodies, where the
coolest one is restricted to having a constant temperature and area
representing the full surface of the neutron star (dashed line in
Figure~\ref{fig:xray}c).  The triangles represent the fluxes from
one or two blackbodies (hot and warm) of much smaller area that
account for the decaying outburst flux.  The squares are the total
flux at each epoch.  It is evident that the fluxes have been steady
since after 2009, just after a slight decrease of $\approx20\%$ in
the hot/warm component between 2008 March and 2009 March.  This
small step-down in flux, corresponding to $\sim8\times10^{32}$
erg~s$^{-1}$ in bolometric luminosity, is the only event in X-rays
that we have been able to find that is approximately coincident
with the turn-off of radio pulsations in late 2008.

\subsection{X-ray and Radio Pulse Phase Alignment}\label{sec:xrayradio}

Five of the X-ray observations listed in Table~\ref{tab:xraylog}
were made during the period in which \xte\ was an active radio
source (see also Figure~\ref{fig:xray}).  For these observations,
we can therefore compare the emission phases of the X-ray and radio
profiles.  For each of these observations (two made with \chandra\
and three with \xmm), we used TEMPO to fit for an offset between
the X-ray TOA and a small number of surrounding radio TOAs (the
latter corrected to infinite frequency using the DM from
Table~\ref{tab:parms}).  The radio reference phase is the peak of
the main radio component, which owing to changing pulse shapes can
contribute up to $0.02\,P$ jitter in this comparison.  The X-ray
reference phase is the peak of the approximately sinusoidal profile,
which has an effective uncertainty of up to $0.1\,P$ for the \chandra\
observations and is a little better for the \xmm\ profiles.

The measured offset between the X-ray and the radio TOAs was, in
chronological order, 0.21, 0.03, $-0.17$, 0.01, and $-0.28$\,s.
All radio and X-ray TOAs therefore match to within $0.05\,P$.  Thus,
at least between 2006 September and 2008 March, the peak of radio
emission coincided with the peak of X-ray emission.

\section{Discussion}\label{sec:disc}

\subsection{Geometry of the Rotating Neutron Star}\label{sec:rvm}

Since the main radio pulse coincides with the peak of the X-ray
emission, it is reasonable to assume that both radio and X-ray are
coming from near the surface, where a hot spot is located at the
footpoint of a bundle of magnetic field lines \citep[for
the other two magnetars with detected radio and X-ray pulsations,
the radio profile is not as well aligned with, but still overlaps,
the X-ray profile;][]{hgr+08,tpe+15}.  In this picture,
currents flowing along this field-line bundle are responsible for
both surface heating and radio emission.  The X-ray and radio pulses
should coincide as long as the field lines are normal to the surface
and the radio emission height is much smaller than the radius of
the speed of light cylinder.  While these are reasonable assumptions
for the open field-line bundle in ordinary pulsars, the geometry
may be different in the case of magnetars, where currents on closed,
twisted magnetic field lines are thought to contribute to X-ray
emission via resonant cyclotron scattering \citep{lg06,ft07}, and
the location of the radio emission region is not obvious.  Therefore,
the rotating vector model \citep[RVM;][]{rc69a} is not necessarily
applicable unless the radio emission is produced on open field lines
as in ordinary pulsars.  Theory and observation are inconclusive
as to whether radio emission in magnetars is produced on open or
closed magnetic field lines \citep{tho08a}.

Assuming that the RVM applies to magnetars, \citet{crj+07} used it
to deduce the geometry of the star.  There were two possible solutions
depending on whether an orthogonal jump in polarization was introduced
between widely spaced pulse components (P1 and P3 in
Figure~\ref{fig:pol}a).  In the first solution, without an orthogonal
jump, the magnetic and rotational axes are almost aligned,
$\alpha\approx4\degr$ and $\beta\approx4\degr$, where $\alpha$ is
the angle between the magnetic and rotation axes, and $\beta$ is
the angle of closest approach of the line-of-sight to the magnetic
axis.  The second solution, with an orthogonal jump inserted, had
$\alpha\approx70\degr$ and $\beta\approx25\degr$.

New data reported here show a polarized component not present earlier
(P2 in Figure~\ref{fig:pol}b and d, at pulse phase between those
of P1 and P3). If we combine all the information on the PA values
from different epochs (namely from data represented in
Figures~\ref{fig:pol}a, b, and d), we obtain RVM fits which are
consistent with those presented in \citet{crj+07}. The result is
again $\alpha\approx4\degr$, $\beta\approx4\degr$ with no orthogonal
jump.  The addition of an orthogonal jump between components P2 and
P3 (see Figure~\ref{fig:pol}b) yields $\alpha\approx67\degr\pm10\degr$
and $\beta\approx16\degr\pm5\degr$.  Broadly speaking, therefore,
the same arguments apply as before --- either the pulsar is aligned,
which is problematic given the X-ray pulse properties discussed
below, or $\alpha$ is large and the emission height, determined
from the width of the pulse, is also relatively large,
$\sim2\times10^4$\,km, about 8\% of the light cylinder radius
\citep[see][]{crj+07}.

It appears that the X-ray spectrum of \xte\ has always been dominated
by the thermal hot spot and surrounding warm region \citep{gh05,hg05},
which is supported by the single-peaked X-ray pulse that aligns
well in phase as a function of energy.  So the X-ray pulse has been
modeled independently of the radio as an indicator of the spin
orientation and viewing geometry of a surface hot spot, which can
then be compared with the results of the RVM fits under the assumption
that the hot spot underlies a perpendicular radio beam.  The most
recent such X-ray modeling results \citep{bpg+11} allow, in our
notation, $\alpha$ in the range $29^{\circ}$--$52^{\circ}$, which
is degenerate with $\zeta=|\beta+\alpha|$, while $\beta$ ranges
from $0^{\circ}$ to $23^{\circ}$.  Their extreme solutions have
$(\alpha,\zeta)=(29^{\circ},52^{\circ})$ or
$(\alpha,\zeta)=(52^{\circ},29^{\circ})$.  Neither of the RVM
solutions are entirely consistent with the model of the X-ray pulse,
although the high pulsed fraction of the harder X-rays would at
least seem to rule out a nearly aligned rotator with $\alpha\sim4\degr$,
and a geometry with $(\alpha,\beta)\approx(52\degr,16\degr)$ seems
reasonably compatible with both radio and X-ray observations.

\subsection{Decline of the X-ray and Radio Luminosity}\label{sec:decline}

A detailed explanation for the exponential X-ray decay of \xte\ was
developed by \citet{bel09}.  In this model, a bundle of closed,
twisted magnetic field lines centered on the magnetic dipole axis
carries the current that heats a spot on the surface.  This so-called
``j-bundle'' is the result of a twist of the crust by the starquake
that initiated the outburst.  As the j-bundle untwists, its boundary
recedes toward the magnetic pole; thus, the area of its footpoint
decreases, which accounts for the declining blackbody area fitted
to the X-ray spectrum \citep{gh07b,bid+09}.

\citet{bel09} also accounts for the non-monotonic change in spin-down
rate of \xte, which after the outburst first increased then decreased
as shown in Figure~\ref{fig:xray}b.  The initial increase in torque
is caused by growing twist of field lines near the magnetic axis,
even as the outer boundary of the j-bundle is shrinking.  This twist
inflates the poloidal field lines, effectively increasing the dipole
moment and the magnetic field strength at the light cylinder.  Once
the twist reaches a maximum stable value of $\sim 1$ radian, the
dipole moment decreases due to the continued contracting of the
j-bundle, and the torque decreases.

In this picture, radio emission is produced on the closed field
lines of the j-bundle, which is wider and more energetic than the
open field-line bundle.  Therefore, radio emission from a transient
magnetar in outburst could be easier to see, both for geometric and
energetic reasons, than in its quiescent state.  Its radio beam
could be broader and different in many respects (spectrum, polarization,
variability) from those of ordinary radio pulsars.  The radio pulse
in this model is coincident with the X-ray pulse, and when the
j-bundle contracts to less than the width of the observed radio
beam, then the radio emission should decrease rapidly.

However, in this model one may expect the width of the radio pulse
to decrease gradually to zero as the j-bundle shrinks, possibly
approaching zero width and disappearing when the outer boundary of
the emitting region reaches the tangent point to the observer's
line of sight.  But this is contrary to the observations, which
show no change in the width or complexity of the radio pulse just
before it disappeared.  The X-ray flux from the hot/warm spot showed
at most a 20\% decrease ($\sim8\times10^{32}$ erg~s$^{-1}$) at the
epoch of radio disappearance, when there was no detectable change
in spin-down power in the X-ray timing.  Since this luminosity
change is comparable to or greater than the spin-down power at the
time, it is difficult to understand how spin power could be responsible
for the event.  Probably a more subtle physical process is required
to explain the sudden quenching of the radio emission.

\citet{rptt12} proposed that the (then) three radio-detected magnetars
share the property that their quiescent X-ray luminosity is smaller
than their spin-down power, but not the converse: not all magnetars
with $L_x/\dot E < 1$ are radio pulsars.  However, review of these
parameters for \xte\ shows that the minimum spin-down power of \xte,
which it reached in quiescence in 2007--2012, is in the range $\dot
E = (5.6-6.6) \times 10^{32}$\,erg\,s$^{-1}$, while its quiescent
(0.3--10\,keV) X-ray luminosity is $L_x \approx 1 \times
10^{33}\,d_{3.5}^2$\,erg\,s$^{-1}$, uncorrected for absorption,
both before and after the outburst \citep{ghbb04,bpg+11,ah16}.  The
distance of 3.5\,kpc is taken from \citet{mcr+08}.  The bolometric
luminosity of the cool component alone from \citet{ah16} is
$4\times10^{34}\,d_{3.5}^2$\,erg\,s$^{-1}$.  These values of $\dot
E$ and $L_x$ disagree with the ones used in \citet{rptt12}, and do
not support their proposition, because the X-ray luminosity of \xte\
is greater than its spin-down power, whether before, during, or
after the outburst.

\citet{smg15} explain radio pulsations from magnetars and ordinary
radio pulsars by a single model, the partially screened gap.  It
assumes that rotational energy heats the open-field-line polar cap,
and the resulting temperature, compared with a critical temperature
for ion emission, is what determines whether a partially screened
gap is maintained.  Only if the luminosity of the polar cap is much
less than the spin-down power is radio emission possible.  However,
the temperature of the X-ray/radio emitting cap in \xte\ is larger
than that of a rotation-powered pulsar with the same timing parameters
because it is heated by magnetic field decay, not by rotation.
During the outburst of \xte\ the polar cap luminosity rose by more
than two orders of magnitude while the spin-down luminosity only
increased by a factor of 8.  So it is not clear how this model could
explain the onset or turn-off of radio pulsations during the outburst
of \xte.

\section{Conclusions}

Radio pulsations appear to be characteristic of some, but not all
transient magnetars in outburst.  The long record left by the single
known outburst of \xte\ provides a prototype for investigating the
mechanism of magnetar radio emission.  The radio flux densities and
X-ray fluxes each declined by about a factor of 50 from
the peak of the outburst to the year 2006.  Then the X-ray and radio
luminosities both levelled off in 2007.  This large-amplitude
correlation would argue that the power for the radio emission comes
from the magnetar mechanism that creates currents in the pulsar
magnetosphere and heats the neutron star crust, rather than from
rotation power.

The radio pulses of \xte\ before they turned off continued to show
large day-to-day fluctuations, unlike ordinary radio pulsars.
The radio spectrum appears to have changed from flat to
steep as the radio (and X-ray) emission leveled off.  The emission
remained highly polarized, and the observation of a new polarized
pulse component allowed us to test and refine the previously derived
emission geometry assuming a dipole field geometry.  This was
compared with independent modeling of the X-ray pulse, which is
coincident in phase with the main radio pulse.  The radio polarization
allows two solutions, depending on whether an orthogonal jump in
polarization is assumed between pulse components.  However, the
almost aligned solution appears inconsistent with the large-amplitude
X-ray pulse, so we favor the more inclined model.

Finally, the radio pulsations turned off abruptly in late 2008, and
have not reappeared in the subsequent 7 years.  However, a continuing
pulse of hard X-rays from a hot spot persists during the radio quiet
epoch and exceeds the spin-down luminosity, evidence of continuing
magnetar activity.   This should not be thought of as a ``return
to quiescence,'' because magnetar activity is not a quiescent state,
but a continuing conversion of magnetic energy to luminosity that,
for a period of years, may well result in a quasi-constant luminosity.
Also, we do not know enough about the pre-outburst state of \xte\
to determine if it had precisely the same emission properties then
as is does now, or if it was truly quiescent prior to the outburst
detected in early 2003.

The sudden radio disappearance prompted us to search for any
contemporaneous event in the X-ray record that could be associated.
The only possible such occurrence was a step-down in the X-ray flux
of the hot spot by $\approx20\%$ between 2008 March and 2009 March.
Although this would appear to be a small effect, it bears some
consideration, as none of the other observations and theories offer
a natural explanation for the sharp radio turn-off.

\acknowledgements

The National Radio Astronomy Observatory is a facility of the
National Science Foundation operated under cooperative agreement
by Associated Universities, Inc.

The Nan\c{c}ay Radio Observatory is operated by the Paris Observatory,
associated with the French Centre National de la Recherche Scientifique
(CNRS).

The Parkes Observatory is part of the Australia Telescope, which
is funded by the Commonwealth of Australia for operation as a
National Facility managed by CSIRO.

This investigation is partly based on observations obtained with
\xmm, an ESA science mission with instruments and contributions
directly funded by ESA Member States and NASA, and with \chandra.
The \chandra\ X-ray Observatory Center is operated by the Smithsonian
Astrophysical Observatory for and on behalf of NASA under contract
NAS8-03060.  This research also made use of data obtained from the
High Energy Astrophysics Science Archive Research Center (HEASARC),
provided by NASA's Goddard Space Flight Center. JPH acknowledges
support from NASA ADAP grant NNX15AE63G.

{\em Facilities:}  \facility{GBT (Spigot, BCPM)}, \facility{NRT
(BON)}, \facility{Parkes (DFB, AFB)}, \facility{CXO (ACIS-S)},
\facility{XMM (pn, MOS)}


text:
Reed Hastings is an American billionaire businessman. He is the co-founder, chairman, and Co-chief executive officer of Netflix, and sits on a number of boards and non-profit organizations.
Howard Marks
Mark Cuban: "Principles is the book I wish I had as a young entrepreneur, stressing over not knowing what I didn't know."
Tony Robbins: "I found it to be truly extraordinary."
Arianna Huffington: "Beautifully written and filled with such wisdom."
Michael Bloomberg: "Ray Dalio's market acumen is legendary, but it was creating and living by a set of principles that allowed him to reach the top. Everyone with goals and dreams can learn from Ray's approach."
Reed Hastings: "Principles had a profound positive impact on my leadership style."
Jack Dorsey: "Principles is helpful in showing people how to operate by clearly articulated and shared principles that lead to faster progress."
Tim Ferriss: "I highly recommend this book. It has already changed how I think about making decisions in my life and in my business, how I think about managing, how I think about managing, how I think about communications between teams."
Kevin Systrom: "I was blown away. It's both a guide to life, a guide to business, and also I think an insight into Ray and someone who's built an amazing business."
Naval Ravikant: "As with most non-fiction, the meat was in the beginning."
7 Powers: The Foundations of Business Strategy
Hamilton Helmer
Daniel Ek
Reed Hastings: "The forces of competition are just incredibly strong. Everyone is trying to eat your lunch, and if you don't read 7 Powers you're going to die a lot sooner."
Peter Thiel: "Hamilton Helmer understands that strategy starts with invention. He can't tell you what to invent, but he can and does show what it takes for a new invention to become a valuable business"
Patrick Collison: "Correctly places enormous value on execution and on culture. However, I think this sometimes leads to insufficient importance being placed on strategy.
Hamilton Helmer's deeply incisive work will hopefully help correct that"
Daniel Ek: "Hamilton Helmer is the best kind of big thinker – he offers great insights that you can turn into real world action.
At Spotify the 7 Powers are widely used as we discuss new initiatives.
His distillation of the key types of strategic power, how to find them, how to leverage them, and how to maintain them is a fantastic toolset for companies at every stage."
One of the books Keith Rabois recommends for entrepreneurs.
Powerful: Building a Culture of Freedom and Responsibility
Reed Hastings: "Magical! An enlightening ride through young companies bucking orthodoxy."
Arianna Huffington: "Patty McCord's compelling account of the culture that made Netflix succeed should be required reading for everyone who wants their business to thrive in the 21st century.
A natural-born storyteller, McCord shows us how the Netflix 'methodology' of radical honesty, debating everything and relentlessly focusing on the future can set us up to win in the 21st century.
With Powerful, McCord challenges, entertains, and inspires as she sets out how we can bring out the best in ourselves and others."
Reed Hastings: "Coming from an industry driven by disruption, it's refreshing to read Brad Smith's call for the tech sector to assume more responsibility.
In Tools and Weapons, Brad and Carol Ann Browne wrestle with some of the world's toughest technology challenges with common sense and valuable insight reflecting their inside experience.
The ideas in Tools and Weapons won't solve all our problems, but they're a very good place to start."
Satya Nadella: "It's an important book on some of the biggest tech issues of our time and their impact on all of our lives – and well worth reading."
Seth Godin: "A book I wish I had written. There aren't many books I haven't written that I wish I had written and this is one of them.
If you care about how ideas spread in our culture and you want to understand issues around scarcity and abundance, about how we pick what we want in an era when the gatekeepers have left the building, well, The Long Tail will help you see it."
Reed Hastings: "It belongs on the shelf between The Tipping Point and Freakonomics."
Beyond Entrepreneurship
Advice for young CEOs from Reed Hastings: "Memorize the first 86 pages of 'Beyond Entrepreneurship' by Jim Collins."
That Will Never Work
Marc Randolph
Reed Hastings: "Engaging and insightful"
Evan Spiegel
Most Recommended Investing Books
Most Recommended Technology Books
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Most Recommended Biographies
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redpajama_set_name: RedPajamaCommonCrawl


text:
Getting Divorced arrow_drop_down
After Divorce Alternatives to Divorce Divorce Advice From the Judge Divorce Basics Divorce Without Court Filing for Divorce Uncontested Divorce
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Alimony Divorce and Property
Home Family Law and Divorce State Divorce and Family Laws Illinois Divorce and Family Law
Illinois Dissolution of Marriage FAQs
Dissolution of Marriage is just another term for divorce.
How is a divorce case started in Illinois?
A dissolution of marriage (divorce) is commenced by the filing of a "petition" (legal paperwork requesting a divorce). The spouse who files is called the "petitioner." The other spouse is called the "respondent."
The respondent spouse must be "personally served" to bring him or her within the "jurisdiction" (authority) of the court; this is also referred to as "service of process" and means that the divorce petition and summons must be personally delivered to the respondent. This may be done by the sheriff or a "special process server" appointed by the court.
The respondent must file an "appearance" with the court, either pro se (representing oneself) or through an attorney.
The respondent (or the respondent's attorney) must file a document known as an "answer" or "response" admitting or denying the allegations of the petition.
What happens if the respondent spouse cannot be located or tries to avoid service of process?
If the respondent cannot be found, a court may still terminate the marriage and enter divorce and custody orders and judgments. However, unless the respondent has been personally served, or has voluntarily filed an appearance, his or her property rights cannot be adjudicated, and no support or maintenance order may be entered.
What happens if the respondent is served, but does not file an appearance or an answer?
A court may find that the respondent is in "default," and the petitioner may be awarded a divorce and such remedies as maintenance(alimony), child support and property distribution.
What steps may be taken while the divorce action is pending?
During a divorce, either spouse may file a petition or motion for "temporary relief," including temporary custody, child support and maintenance. After a hearing, the court may enter temporary orders, which will remain in effect until they are modified (changed) by a court, or until the final judgment for dissolution is entered.
How does the judge know who is right or wrong?
Both parties are required to provide information and documents under oath concerning any issue relevant to the case. If there is a dispute over custody or visitation, the parties may be ordered to mediation and/or for evaluation by custody experts. The court has statutory power to appoint an independent expert to conduct an investigation and make recommendations. The parents may also seek evaluation of the children and each other by their own partisan experts. The judge has discretion as to whether or not to interview the children in camera (in chambers). The judge will hold hearings or a trial at which both parties present testimony and other evidence. The judge is required to make his or her decisions based upon the law and the evidence.
Can children have their own lawyer?
An attorney and/or a guardian ad litem (GAL) may be appointed by the court to represent the children. A concerned parent may request appointment if the children's interests are likely to get buried in the parents' issues. Where the parents are acrimonious, the judge may simply decide to make the appointment.
Who pays for the child's attorney?
The parents will be required to pay the fees of the child's court-appointed representative unless they are without means to do so, in which case a public attorney may be appointed. The judge will allocate the fees between the parents, based upon their relative ability to pay. A parent may not hire a lawyer to represent the children. However, the attorneys for the parents may agree to a representative for the children, and the judge will usually go along with the attorneys' joint recommendation. The attorney for the child or GAL has considerable power and influence in the outcome of the case for the children.
Is there a right to a jury in divorce cases?
No -- there is no jury in divorce or custody cases in Illinois.
Is there a trial in every case?
No. Most family law cases are settled, sometimes after several years of interim wrangling and court proceedings, and after expenditure of many thousands of dollars which could have been divided by the parties for the good of the family. The few cases that are not settled go to trial before a judge, and all rules of procedure and evidence applicable in any civil lawsuit will be applied.
If a party thinks the judge is wrong, does he or she have any recourse?
Yes. A party who is unhappy with the outcome of a divorce trial has a right to appeal. However, appeals are very costly. ($10,000 for each party is not an unusual figure.) Illinois law gives the trial judge a lot of discretion, and appeals are not always successful.
If you have questions about a divorce in Illinois, you should contact an experienced family law attorney in your area.
For more information on dissolution of marriage, see Divorce Basics in Illinois, by Yan Wen Fei, in our Illinois Divorce and Family Law section.
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Rainbows are glorious, even if more clouds gather | Lowry
Pride Month shows how the LGBTQ community, 50 years after the Stonewall riots, continues to flourish in the face of violence and intolerance.
Rainbows are glorious, even if more clouds gather | Lowry Pride Month shows how the LGBTQ community, 50 years after the Stonewall riots, continues to flourish in the face of violence and intolerance. Check out this story on northjersey.com: https://www.northjersey.com/story/opinion/columnists/2019/06/07/rainbows-glorious-even-if-more-clouds-gather-lowry/1372253001/
Bruce Lowry, North Jersey Record Published 4:43 a.m. ET June 7, 2019 | Updated 4:02 p.m. ET June 7, 2019
Last week in Rutherford, they ran the rainbow flag up the flagpole for the first time.
"By raising this flag today, we begin to reinforce the message of love and acceptance, that all people, no matter who they love or who they are, are welcome within our town," said Rob Lyons, chairman of the Rutherford Pride Alliance. "Our wish is that anyone that sees this flag raised will know that we will not stand for intolerance or hate."
The rainbow flag, known as the pride flag, is recognition that a given community has fully embraced its lesbian, gay, bisexual, transgender and queer residents, as well as those LGBTQ travelers who may be stopping through, for a coffee or a bagel, or to visit an old friend.
More than anything, the pride flag says: "Welcome; we are glad you came our way."
Yet our world being what it is, there are sometimes darker clouds beyond the rainbow. There are still places where some people, for whatever reason, are not welcome.
For every Rutherford, or Glen Rock, or Ridgewood, there is a Carbon Hill, Alabama.
The day before the Pride Month celebrations that were such joyous occasions all over North Jersey, the mayor of Carbon Hill, in what was once known as part of Alabama "coal country," was spewing forth the sort of hate-filled ignorance and nonsense that keeps this nation from stepping full forward into the 21st century.
The 49th annual Pride Parade was held in New York City on Sunday, June 24, 2018. The parade commemorates the Stonewall Riots that erupted in response to a police raid of the gay bar the Stonewall Inn in the Greenwich Village neighborhood on June 28, 1969. The parade marks the end of Pride month. (Amy Newman/@2amyb) (Photo: Amy Newman/@2amyb)
And to those who recall the bus burnings, the church bombings, and "Bull" Connor's dogs and fire hoses that were emblematic of Alabama in the 1960s, the words posted by Carbon Hill Mayor Mark Chambers were all too reminiscent of another time, when another group of people were targeted because of their skin color.
In case you are just catching up to the Carbon Hill story, in a now-deleted Facebook post, Chambers ranted about "a society where homosexuals lecture us on morals, transvestites lecture us on human biology, baby killers lecture us on human rights and socialists lecture us on economics."
This moved a friend of Chambers to respond in kind: "I hate to think of the country my grandkids will live in unless somehow we change and I think that will take a revolution."
To that remark, the good mayor replied, in part, "without killing them out there's no way to fix it."
Since then, Chambers has offered an apology of sorts, and maintained that although he "was not targeting the LGBTQ community, I know that it was wrong to say anyone should be kill."
One more public official "apologizing" after writing or saying something highly offensive, if not threatening, and being called out for it. Backlash toward Chambers has been furious, with some calling for him to resign, and others saying he was "inciting violence."
The glory of Pride Month is that it shows how the LGBTQ community, 50 years after the Stonewall riots in Manhattan, continues to flourish in the face of violence and intolerance, and continues to demand its rightful place in a nation that is supposed to be all about individual freedoms.
More: Rutherford raises its first LGBTQ flag as towns throughout Bergen County mark Pride Month
More: If Rutgers loses The Daily Targum, its students lose a champion | Lowry
In recent days, we rightly paid tribute to those who made the ultimate sacrifice in defense of those freedoms on the beaches of Normandy during World War II.
It is worth reminding, however, that some basic freedoms are still being defended, in this country and around the world.
Certainly, some minds, some core beliefs, may never change.
That doesn't mean we should give up. It means we should continue to strive to educate and to articulate the need for greater understanding.
The folks who raised the rainbow flags last weekend had the right idea. They stand on the right side of history, and stand firm even in the knowledge that their stance will be challenged.
Those who seek common decency and basic rights have been challenged before. They know what it takes to ride out the storm.
Bruce Lowry is the editorial page editor for The Record and Northjersey.com. Email: lowryb@northjersey.com
Read or Share this story: https://www.northjersey.com/story/opinion/columnists/2019/06/07/rainbows-glorious-even-if-more-clouds-gather-lowry/1372253001/
Opinion: Time to repeal religious exemption from vaccines
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The bond between blacks and Jews must remain strong | Opinion
Standing up for the poor, once again | Editorial
Editorial: NJ must address its addiction to road salt in winter


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John (given name)
John (Lil Wayne song)
John is a common English name and surname:
John (given name) or
John (surname), including a list of people so named
John may also refer to:
People with the given name
John Hyrcanus, ruler of Judea 134–104 BC
John the Baptist (c. 7 BC – c. 30 AD), regarded as a prophet and the forerunner of Jesus Christ
John the Apostle (c. 6 – c. 100 AD), one of the twelve apostles of Jesus
John the Evangelist, alleged author of the Fourth Gospel, traditionally identified with the Apostle
John of Patmos, the Seer of the Book of Revelation, traditionally identified with the Apostle
John the Presbyter, an obscure figure either identified with or distinguished from the Apostle, the Evangelist and John of Patmos
This page contains text from Wikipedia, the Free Encyclopedia -	https://wn.com/John
John /dʒɒn/ is a masculine given name in the English language. The name is derived from the Latin Ioannes and Iohannes, which are forms of the Greek name Iōannēs (Ἰωάννης), originally borne by Hellenized Jews transliterating the Hebrew name Yohanan (יוֹחָנָן), "Graced by Yah", or Yehohanan (יְהוֹחָנָן), "Yahweh is Gracious". There are numerous forms of the name in different languages; these were formerly often simply translated as "John" in English but are increasingly left in their native forms (see sidebar).
It is among the most common given names in Anglophone and European countries; traditionally, it was the most common, although it has not been since the latter half of the 20th century. John owes its unique popularity to two highly revered saints, John the Baptist (forerunner of Jesus Christ) and the apostle John (traditionally considered the author of the Gospel of John); the name has since been chosen as the regnal or religious name of a vast number of emperors, kings, popes, and patriarchs. Initially, it was a favorite name among the Greeks but it flourished in all of Europe after the First Crusade.
This page contains text from Wikipedia, the Free Encyclopedia -	https://wn.com/John_(given_name)
"John" is a song by American rapper Lil Wayne, and the second single from his album Tha Carter IV. The song features rapper Rick Ross, and it peaked at number 22 on the Billboard Hot 100. "John" was released on March 24, 2011, on iTunes. The song uses the hook from Rick Ross' song "I'm Not a Star" from his album Teflon Don. The song title refers to musician John Lennon. Lil Wayne performed the song at 2011's MTV Video Music Awards to the riff of Black Sabbath song, Iron Man.
The music video was released on VEVO on May 12, 2011. Birdman makes an appearance in the video, which was directed by Colin Tilley, who directed Chris Brown's "Look at Me Now," which also featured Wayne.
On May 11, rapper Ace Hood released a freestyle over the beat of "John," which was off his "Body Bag Vol. 1" mixtape. Another rapper Wiz Khalifa released a remix to "John" titled "Chuck". Rapper Chamillionaire freestyled a verse along with the original lyrics on his Badass Freemixes 2 mixtape. On December 26, Lil Wyte also released his own version on his Wyte Christmas mixtape. Tyga also released a version of the track titled "Well Done 2" on a mixtape along with the same name. Jim Jones also released a freestyle.
This page contains text from Wikipedia, the Free Encyclopedia -	https://wn.com/John_(Lil_Wayne_song)
Bankson, John Filmography
2010, role: actor , character name: Alexander Gardner
Hot Shots!
1991, role: actor , character name: Parking Valet
1989, role: actor , character name: Monster Referee
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Latest News for: john bankson
Selectmen races on ballot in Ipswich, Middleton, Boxford
The Salem News 19 May 2019
May 21 is Election Day in Ipswich, Middleton and Boxford ... to 8 p.m. Middleton ... Town Clerk Robin Phelan, Boxford School Committee member Elizabeth Palmer, Board of Health member Alexander Constan, Board of Assessors member David Benson, Planning Board member John Adams, library trustee Jayne Smallman, and trust funds commissioner Bankson Riter Jr ... ........
On the market: Historic John Palmer house with garden oasis for $1.15 million
Philadelphia Daily News 17 Apr 2019
Deborah Khan and her husband, Nasir, had been living in a Queen Village trinity when they bought their four-bedroom Society Hill Home. "We needed more space, and I was always interested in history," Khan said. The 2,779-square-foot property was built in 1743 by bricklayer John Bankson Palmer ... "It's so amazing." ... "We've put a lot of ourselves into it."....
LETTER TO THE EDITOR: Vote in favor of school referendum
SCNOW Morning News 27 Jan 2019
Economic development is not just about job creation and investment; it is also about raising the standard of living and improving the community and quality of life for all of our citizens ... John Bankson, Joan Billheimer, Buddy Brand, Jamie Carsten, Darryl Hall, Jill Lewis, Jeff Payne, Buzz Rogers, Jumana Swindler, James Tolston and Nick Townsend .......
Brand: Area benefits as Florence County grows
FLORENCE, S.C. – Florence County's capital investment for the 2018 fiscal year was approximately $89.17 million, and 521 jobs were created ... In his report, Brand said Florence is growing, and that is exciting ... "STEM Premier completes the cycle," he said ... 4 ... They are Jill Lewis, chairman; Billheimer, vice chairman; and John Bankson, treasurer ... .......
Doane University awards degrees to area students
The Grand Island Independent 27 May 2018
... Gabriel of Hastings, master of arts in management; Ryan Kern of Hastings, bachelor of arts in business administration; Lisa Smith of Hastings, doctorate of education; Adam Story of Hastings, master of arts in management; John Yandell of Hastings, master of arts in management;....
Florence Little Theatre recaps the season, hands out awards
SCNOW Morning News 26 May 2018
FLORENCE, S.C. – The Florence Little Theatre held its 55th annual Awards Night on Thursday evening ... The winners. ... The night ended with the passing of the gavel from Thompson to incoming President John Bankson, followed by a video preview of the 2018-19 season lineup, which kicks off in July with "Aladdin, Jr." .. .......


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The California areas inside the space code 760 are:
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Home Contact | Site Search:
South Dublin County History
Stair Chontae Atha Cliath Theas
OUR VILLAGES
Clondalkin - History
Clondalkin - Cluain Dolcain - Dolcan's Meadow is located on the banks of the River Camac. Situated on the heights over the estuary of the River Liffey it guards the inland pass between the mountains and the river. This advantageous location first attracted Neolithic settlers around 7,600 years ago. The presence of the Celtic tribe of Cualann, who settled in this area, is recorded by the many mounds and raths which they left behind.
Christianity came to East Leinster in the 5th century. Its foundation at Clondalkin is ascribed to St. Cronán also known as Mochua. The monastery was situated where St. John's Church now stands and as was the practice it was surrounded by a protective fosse, the outline of which can be followed in today's village streetscape. Orchard Road, with the gardens sloping up from road level, formed the boundary on one side. Continuing along the Main Street it then curved to the west of the Round Tower.
Saint Cronán Mochua died in 630 AD. His feast day is celebrated on the 6th of August. Evidence that the foundation continued after St. Mochua's death is confirmed as the names of Abbots and the Bishops of Clondalkin were recorded until 1080 AD.
Visible from all directions, the dominant feature of Clondalkin Village is its Round Tower. Unfortunately no records exists which indicate when it was built. The purpose of Ireland's round towers has long been a matter of debate. In 1725, the first historian to concentrate on these towers was Dr.Thomas Molyneaux. He argued that they were of Danish origin. However in 1833, George Petrie, in an essay for the Royal Irish Academy, refuted these suggestions stating that the towers were the symbolic central feature of the early Celtic Church. It is now accepted that a round tower - Cloig Theach in Irish, was used as a Bell Tower and to safeguard the relics of a monasteries founder.
The Annals of Ulster record that the relics of St. Kevin and St. Mochua were taken on tour in 790 AD. It is thought that the Clondalkin Round Tower was built around this period. Certainly it is of a very early type with rough calp limestone used in its construction. There are no signs of any of the stones being shaped by a mason. The door and window frames are formed from Leinster granite erratics.
The Clondalkin Round Tower is 27.5M high and is complete with its original cap. With a circumferences of 12.7M above the buttress, it is the most slender of all Round Towers. The buttress at the base is not original and there is no record to indicate when it was added. This buttress appears in a 1725 drawing by Samuel Molyneaux.
Norsemen invaded in 832, 1071, and again in 1076 AD when they settled in the area. They built a fortress and named it Dun Amhlaeibh after their King. The village came under the control of the Archbishop of Dublin and by the 13th century Clondalkin was described as a town with many inhabitants. The town was ruled by a bailiff and in 1276 we know that a Robert Beg held this position. There was also a weigh master in the village. This was due to the importance of trade.
From an inquisition, regarding property assigned in 1393 to the Church of Clondalkin by one John Shillingford, we know that there were at least five streets in the village namely: Mahow Street; Mill Street; New Street; Steeple Street and Pope Lane.
Clondalkin was established as a borough in 1300 and in 1547 it was recorded that:
"Clondalkin is among the walled and good towns of the County"
The present St. John's Church was opened in 1789. It had an open belfry and 12 seats. Restoration, which started in 1834, gave us the Church of Ireland structure we see today. The medieval church which stood on this site was demolished in 1787 to allow work to start on a new church. There are no records stating when this church was built yet according to Dr. Petrie it was a church of considerable architectural importance and was probably built during the 13th Century.
The earlier church measured 120 feet long and 50 feet wide. The church was dedicated to St. Mochua and contained three altars honouring Mary the Blessed Virgin; St. Bridget and St. Thomas. All that remains of this earlier church is a column of stonework in the churchyard.
There are two early crosses in the graveyard, a larger granite cross which was possibly a boundary cross for the Barony of Uppercross, of which Clondalkin is a part and a smaller carved cross. Another item of note is a large baptismal font carved out of a granite erratic.
St. John's graveyard was the village graveyard where burials from all denominations occurred for a long period. There are many interesting tombstones within the graveyard including those of two Catholic Parish Priests along the back wall.
On Sunday the 8th of March, 1857, the Parish Priest Fr. Moore held a parochial meeting in the Chapel House. He proposed the erection of a new church. It is recorded that his suggestion was responded to "in a manner unprecedented in the Annuals of Chapel building in Ireland". Certainly a large sum of money was pledged with many parishioners subscribing £50 to £100 each.
The Church of the Immaculate Conception was designed by F. W. Caldbeck in the Gothic style and the foundation stone was laid on Sunday the 5th of July 1857, by His Grace the Most Rev. Paul Cullen, Archbishop of Dublin. In a container placed under the stone were coins of Pope Pius IX and of Queen Victoria, along with an inscribed parchment. The church organ was installed by Messers Telford and first played on 12th May 1867. On that occasion, the organist was Professor Glover, organist in Dublin's Pro-Cathederal. The choir comprised of the Pro-Cathederal choir with the principal singer Madame La Vega Wilson and the Presentation Convent Choir.
Clondalkin is regarded as a centre for the Irish language and culture. Munitir Cronáin was founded in 1972 to further the use of the Irish language through educational, social and cultural activities. For many years Muintir Cronáin operated from members' houses and various halls around the village. In May 1989 they purchased Orchard House in the centre of the village and renamed it. Áras Cronáin opened it as a cultural and heritage centre.
In 1975 and again in 1988, Muintir Cronáin was awarded the Glór na nGael National Trophy in recognition of its efforts to promote the Irish language. In 1991 they were chosen to host An tOireachtas - the yearly National Cultural Festival.
More recently, in the mid 1990s the opening of the Mill Centre on the site of the old paper mills and the offices for South Dublin County Council have provided a new focus and purpose to Clondalkin.
Jointly funded by South Dublin County Council and The Department of the Environment, Heritage and Local Government from the Information Society Fund.


text:
Q: how to use in clause into inner join I need a query like that ;
select a.*, b.column1 from table1 a
inner join table2 b on (b.id in (id_array))

This query returns nothing.
What I want to do: I retrieve the group of ids from table1.Then get the name column of these ids from table2. So, I use inner join for this.

A: Shouldn't just be the join?
select a.*, b.* from table1 a
inner join table2 b on b.id = a.id

A: select *
from table1, table2
where find_in_set(id, ids) > 0

A: select a.* , b.* from table1 a inner join table2 b on a.id = b.id

A: I assume that a.ids is some kind of id list, so you could use the find_in_set() function:
select *
from table1 a
join table2 b on find_in_set(b.id, a.ids) > 0

redpajama_set_name: RedPajamaStackExchange


The Academy embraces a philosophy of inclusion in every aspect of our operation, from menu planning to finances. In essence, Academy members have Voice and Choice in program development and decision-making. An inclusive process for hiring Academy staff is a perfect example of how we put this philosophy into practice.
Members and staff share steps that include a working interview for candidates and a "panel interview." Imagine being interviewed by 12 people! Afterward, members and staff come together and make a decision on based on consensus. As you might imagine, it can be quite an accomplishment to be hired by the Academy. The successful candidate will need to get the nod of approval from our community. We are currently interviewing candidates to fill a new opening in our Culinary Team. Stay tuned for updates!


You searched for subject:(Complentarity). One record found.
1. Kalembera, Sylvester A. The implementation of international criminal law in Malawi .
On 17 July 1998, a total of 120 States, including Malawi, voted for the adoption of the Rome Statute of the International Criminal Court. The ermanent ICC became operational on 1 July 2002. The ICC has jurisdiction over the crime of genocide, crimes against humanity, and war crimes. These crimes are the most serious crimes of international concern. The ICC operates under the principle of complementarity, which entails that the ICC will only assume jurisdiction over these core crimes in the event that a State Party is unwilling and unable genuinely to carry out the investigation and prosecution. States Parties have, therefore, the primary responsibility to investigate and prosecute these crimes. The States Parties must therefore establish jurisdiction to conduct investigations and prosecution of these core crimes. It is from that background, coupled with the historical evolution and development of international criminal law, with regard to individual criminal responsibility, that this paper argues for the implementation of the Rome Statute in Malawi, through domestic legislation.The paper thus argues that only through domestic legislation can the purports of the Rome Statute be achieved and fulfilled by Malawi. Advisors/Committee Members: Werle, Gerhard (advisor).


text:
Showing growth: The youngest SCS students improved in literacy this year
Shelby County Schools students in grades three through five made gains in both math and English language arts in TNReady testing.
Showing growth: The youngest SCS students improved in literacy this year Shelby County Schools students in grades three through five made gains in both math and English language arts in TNReady testing. Check out this story on commercialappeal.com: https://memne.ws/2uzUnij
Jennifer Pignolet, Memphis Commercial Appeal Published 2:15 p.m. CT July 19, 2018 | Updated 12:47 p.m. CT July 20, 2018
May 19, 2018 - Whitehaven High School students participate in the school's 2018 graduation ceremony at the Cook Convention Center.(Photo: Brandon Dill for The Commercial Appeal)Buy Photo
The youngest Shelby County Schools students who take state tests made gains in reading last year, according to newly released TNReady data from the 2017-18 school year.
The district made nominal gains in other areas, including elementary math, but results took a few steps back or remained flat in areas like high school English and math.
"We have a lot of positive signs here, things teachers and school leaders can be proud of, evidence we're moving in the right direction," SCS Superintendent Dorsey Hopson said.
On the elementary English language arts test, 23.9 percent of students in grades three through five tested proficient in the subject. That's an increase of 3.1 percentage points from last year.
Students in those grades also increased proficiency in math, up 2.8 points to 28.6 percent.
The gains come a year after SCS made curriculum changes, implementing Eureka Math the Expeditionary Learning reading program.
Hopson noted the district experienced challenges rolling out the changes, including delays in acquiring the necessary materials and resistance from teachers who were concerned they would have to teach to a script.
"I think we've got buy-in now," he said.
Mendell Grinter, executive director of the Campaign for School Equity, said he sees the push at the elementary level having an impact on the scores.
"I feel like I can see that as being responsible," he said of the new reading curriculum.
Overall, Grinter said he was pleased to see the bright spots, but concerned about an overall lack of growth, and in some cases a step backward.
Just 18.9 percent of students in grades six through eight were proficient on the English language arts tests, a slight drop from last year. On math, 16.6 percent of students were proficient, up less than a full point from last year.
High school students in the district saw a larger drop in English, down four points to 15.7 percent. In math, they made a slight gain of 1.6 percentage points, up to 9.1 percent proficient.
Across the state, in high school English, 29.4 percent of students were considered proficient in the subject, down from 34.6 percent in the 2016-17 school year.
SCS this fall will put reading specialists, a position normally found in elementary schools, in middle and high schools. That was already baked into the budget before the state released the test results, but the scores show the strong need, Hopson said.
"I think the state results and our results provide more evidence or more justification for the approach that we're going to take," he said.
In high school math, 22.5 percent were proficient, up from 21.5 percent in the 2016-17 year.
Test results won't count against students, teachers or schools this year after failures with the online system used to administer the test. Only high schools and some middle schools took the test online.
Hopson has spoken out previously with concerns about the validity of the results as a result of the testing issues.
Tennessee Education Commissioner Candice McQueen said Thursday that a third-party analysis showed there was minimal impact on scores, but acknowledged there was no way to quantify a lack of effort form students once they learned the test wouldn't count.
Hopson said he heard from teachers and students that motivation was hard to come by once it was clear a bad test score would do no harm.
"I think we'll never know what the real impact is, but we have to accept the data that came from these tests," he said.
The state will release results for individual schools at a later date.
Plenty to learn: TNReady scores won't count, but here's what you can still learn about your school
Read or Share this story: https://memne.ws/2uzUnij


Is it is well known saying that "actors are born, not made". But the modern day acting schools have altered the saying by proving that actors can also be made. The acting institutes are flourishing in a rapid way in different nations of the world. In India also, there are numbers of acting schools that teach the students the acting skills. The boom in the film and entertainment industry all over Indian metro cities like Delhi, Mumbai, Bangalore, Pune, Chennai and Hyderabad, is making an impact on a large number of youth in the country. If a student wishes to join this industry and work on screen, acting schools can make the path easy for them.
It is not that students can only work as an actor after the completion of the course, they also can set up their own schools so that other students can also learn the skill. In India, a number of acting schools are there among which the Film and Television Institute of India is counted as the best. It is a government approved institute and is among the most famous acting schools of the world.
Acting is a form of performing art. Thus it requires passion, enthusiasm and self esteem from the people who want to turn up to be an actor. One can take admission either in a graduation or post graduation diploma course in acting. There are also short term acting courses available in different institutes. To do a diploma in acting, the students need to complete their senior secondary level. They also have to appear for a written and aptitude test before getting the admission.
The job prospects of the students passed out from an acting school is also very high. The entertainment industry is one of the most flourishing industries in the world. Thus entering into it could be a good choice for the youth. Moreover, in an acting school, the students are also taught about the different aspects of film and television production. The entertainment industry provides a range of opportunities and career choices for every talent.
A tremendous level of potential exists if one has the ability and enthusiasm to grow. Moreover, the students are also given practical knowledge about acting as in every acting school there are acting studios. Besides name and fame, hefty sums of money are assured for a successful actor. India has the distinction of being the largest producer of film producers and financiers who make quality films having global competence.