text:
\section{Introduction}\label{sec_intro}
Rotating radio transients (RRATs)
are a recently discovered class of neutron stars.
At a wave band $\sim$1.4 GHz,
they have sporadic radio pulses
of durations ranging from 0.5 to 100 ms
with flux densities
from $\sim$10 mJy to $\sim$10 Jy
and burst rates
from 0.3 to 50.3 per hour.
The study of the time of arrival (TOA)
of single pulses
indicates that these RRATs have periods
ranging from 0.1 to 7 s
and surface magnetic field
of $\sim$$10^{12}$ or $\sim$$10^{13}$ gauss
\citep{mll+06,dcm+2009,mlk+09,bb2010,kle+2010}.

J1819$-$1458 is the brightest
and most prolific
radio transient
among the more than forty known RRATs.
The dispersion measure of the source is
$DM\approx196$ \dmu.
At 1.4 GHz,
the durations of most bursts are
$\sim$3 ms at intervals of
$\sim$3 minutes
and the peak flux density
is $\sim$10 Jy \citep{mll+06,esamdin+08,lmk+2009}.
The irregular bursts cannot be detected
by standard periodicity search methods,
but a single pulse TOA analysis
is capable of identifying
the rotation period of $P\approx4.26$ s
with a spin-down rate
$\dot{P}\approx5.76\times 10^{-13}$ \mbox{s s$^{-1}$}.
The inferred surface magnetic field density
is $B_\text s\approx5\times10^{13}$ gauss
and characteristic age
is $\tau_\text c\approx1.2\times10^5$ years
\citep{mll+06,esamdin+08}.
\citet{lmk+2009} reported two unusual glitches
with quite different post-glitch behavior
and an associated increase in the flux intensity,
which implies
that RRAT J1819$-$1458
may be moving toward
the death line
in the pulsar $P-\dot P$ diagram.
The Faraday rotation measure
of RRAT J1819$-$1458 is
$RM\approx330\pm30$ \mbox{rad m$^{-2}$}
and the integrated linear polarization measurement
is relatively low
owing to orthogonal modes of polarization,
although some individual pulses are highly polarized
\citep{khs+2009}.

After the {\em{Chandra~X-ray~Observatory}}
detected the X-ray counterpart
\citep{rbg+2006,gmr+2007},
the {\em{XMM-Newton}} discovered
the X-ray pulsation aligned
with the phase of the radio pulse and
a possible X-ray spectral feature that is similar
to those of the X-ray dim isolated neutron stars
\citep[XDINS, cf.][]{ptp06,hab07,kml+2009}.
This indicates that
RRAT J1819$-$1458 is a cooling neutron star and
possibly a transitional object between the pulsar
and magnetar classes (\citealt[][]{mrg+07};
for descriptions of magnetars,
see \citealt{wt06,mer2008}).
\citet{rmg+2009} found the X-ray extended emission
around RRAT J1819$-$1458,
which can be interpreted as being
a nebula powered by the pulsar.
The near-infrared counterpart
to the extended X-ray emission
was not detected
in the observation taken by \citet{rct+2010}.
There is no evidence of the optical counterpart
to the RRAT in the observation implemented by
\citet{dml2006},
but there is possibly
a near-infrared counterpart \citep{rct+2010}.

\citet{wsr+2006}
assumed that some RRATs could be explained
in terms of normal pulsars
that have pulse amplitude modulations,
such as PSR B0656+14.
Had they been put at properly large distances,
their weak pulses would have been undetectable
and they might have been identified as RRATs.
From the observation results
of PSR J1119$-$6127
with magnetic field strength
and post-glitch behavior
similar to those of
RRAT J1819$-$1458,
it is understood
that some RRATs can be interpreted
as the consequences of
the line of sight
missing the steady pulse components
of emission area
and intercepting these unstable ones
\citep{wje2010}.
\citet{wmj07} proposed
that RRATs could not be directly
related to nulling pulsars
because the latter
have no observed pulses
such as giant pulses
\citep[e.g.][]{hkw+03,kbm+06}.
However,
taking PSR J0941$-$39
as an example,
\citet{bb2010} argued
that there was possibly
a link between RRATs
and pulsars
with nulling phenomena.
There is also a hypothesis that
some RRATs are possibly related to
radio pulsing magnetars such as XTE J1810$-$197
\citep{ssw+2009}.
By studying the birthrates of neutron stars,
RRATs have been considered distant XDINS \citep{ptp06}
or an evolutionary stage
of a single class of objects \citep{kk2008}.
In the $P-\dot P$ diagram,
the periods of known RRATs
cover a large range
where periods
of normal pulsars
and magnetars
distribute;
the observational characteristics of RRATs vary
with diversities \citep{mlk+09}.
Although there have been several theoretical interpretations
of RRATs \citep[e.g.][]{li06,zgd07,lm07,cs2008,olny2009},
RRATs do not appear to be completely understood.

This paper presents a study of individual bursts detected
in single pulse observations from April 2007 to April 2010.
Section \ref{sec_obs} describes the observation details.
The results of study on detected pulses
are given in Sect.\ref{sec_res}
and discussed in Sect.\ref{sec_dis}.
Section \ref{sec_con} briefly summarizes this paper.

\section{Observations}\label{sec_obs}
Observations were performed
using the Nanshan 25-m radio telescope of Urumqi Observatory.
The antenna has a cryogenic receiver
of two orthogonal linear polarization channels
with a central frequency of 1541.25 MHz.
Each polarization channel
consists of
128 sub-channels
of bandwidth 2.5 MHz
and has a total bandwidth of 320 MHz.
The signal from each sub-channel is 1-bit sampled
and recorded to hard disk for subsequent off-line processing
\citep[for more details of the system, see][]{wmz+01}.
The minimum detectable flux density
$S_\text{min}\approx3.4$ Jy is limited by
\begin{equation}\label{equ_Smin}
S_\text{min}=\frac{2\alpha\beta{kT_\text{sys}}}{\eta{A\sqrt{n_\text p\tau{\Delta{f}}}}},
\end{equation}
in which $\alpha=5$ is the threshold signal-to-noise ratio (SNR),
$\beta=\sqrt{\pi/2}$ is the loss factor due to 1-bit digitization,
$k$ is the Boltzmann constant,
$T_\text{sys}=T_\text{rec}+T_\text{spl}+T_\text{sky}\approx32$ K is the system temperature,
$\eta\approx57\%$ is the telescope efficiency at 1541.25 MHz,
$A=490.9$ m$^2$ is the telescope area,
$n_\text p=2$ is the number of polarization channels,
$\tau=0.5$ ms is the sampling interval,
and $\Delta{f}=320$ MHz is the total bandwidth \citep{mlc+2001}.

From Apr 10, 2007
to Apr 13, 2010,
260 hours of data were accumulated
in 1100 days of observations.
The time-span of each observation session
was 2 hours.

\section{Data analysis and results}\label{sec_res}
Pulsed radio waves propagating through
the ionized plasma of the interstellar media
are dispersed because
the group velocity in the media
is frequency dependent.
This demonstrates
that the higher frequency components
of a radio pulse arrive
before those at lower frequencies.
To achieve a higher SNR and narrower
(normally closer to the real) profile of the pulse,
the time delay must be removed.
The time difference between the two components
of different frequencies, $\Delta{t}$,
is given by
\begin{equation}\label{equ_dt}
\Delta{t}=4.1488\times{DM}\times(\frac{1}{f^2_\text l}-\frac{1}{f^2_\text h})\textrm{ ms,}
\end{equation}
where $DM$ is the dispersion measure in \dmu,
and $f_\text l$ and $f_\text h$ are the values (in GHz)
of the lower and higher frequencies, respectively
\citep[][Appendix 2.4]{lk05}.
We use Eq.\ref{equ_dt}
with the nominal DM value of
$DM=196$ \dmu~to calculate
and remove the delayed time of signal
between the sub-channel at the lowest frequency
and sub-channels at other frequencies,
finding that the signals
from two polarization channels
are de-dispersed.
The signals of all 256 sub-channels are summed,
and signals of $SNR\ge5$ are searched for
in the whole time series of each observation.
Selected signals
with SNR above the threshold
are reprocessed with $DM$
varying from 0.7 to 300.7 \dmu~in steps
of 1 \dmu.
To each $DM$,
the SNR of the bin with the maximum amplitude is
computed over 1024 bins (512 ms),
with the candidate burst being at the center of the series.
Through the process,
a diagnostic plot shown in
Fig.\ref{fig_gray}
is generated and used for careful inspection
by eye to identify real bursts
\citep[for more details of the burst detection method adopted, see][]{esamdin+08}.

\begin{figure}
\resizebox{\hsize}{!}{\includegraphics[angle=270]{15953fg1.ps}}
\caption{Diagnostic plot showing detected burst
from RRAT J1819$-$1458 and RFI signal.
The upper-left panel is a DM-time gray map generated by
de-dispersing the signal with $DM$ varying
from 0.7 to 300.7 \dmu~in steps of 1 \dmu.
The brightness of the plot
indicates the amplitude
at the corresponding position,
and, the two bright marks at around
$DM=195.7$ and $DM=0$
\dmu~represent the burst and RFI.
The upper-right panel is a DM--SNR graph
with two peak SNR values at around $DM=195.7$ and $DM=0$ \dmu,
in which the SNR for each $DM$ is calculated
from the bin of maximum amplitude over 512 ms.
The lower-left panel is a time series graph
showing the amplitude (in an arbitrary unit)
of each bin at $DM=195.7$ \dmu,
which clearly delineates a narrow burst profile at the center.}
\label{fig_gray}
\end{figure}

In the upper-left panel
of Fig.\ref{fig_gray},
we present a DM-time gray map
that obviously shows two white marks.
The mark at around
the intersection point
of the line of $DM=195.7$
\dmu~and center line of the time series
represents a burst detected
from RRAT J1819$-$1458,
and the one at about 210 ms around $DM=0$
\dmu~represents a signal of
radio frequency interference
\citep[RFI, see][]{cm03}
that sometimes contaminates
the observation data.
The mark representing the burst dissolves
as the $DM$ increases or decreases
from the nominal $DM$,
whereas the one representing the RFI dissolves
as the $DM$ increases from 0 \dmu.
The upper-right panel is a DM--SNR line graph
illustrating the SNR variation with DM,
where the SNR is
from the bin of maximum amplitude
in the 512 ms time series
for every DM value.
As illustrated,
the SNR has two peak values
at around $DM=195.7$ \dmu~for the burst
and $DM=0$ \dmu~for the RFI,
and far away from these two DM values,
the SNR varies like white noise.
The lower-left panel shows the time series
at $DM=195.7$
\dmu~and clearly displays a burst profile in the center.
A typical burst detected
from RRAT J1819$-$1458 has
the visual characteristics
presented in Fig.\ref{fig_gray},
which is a significant criterion
for identifying a real burst.

Using the above method,
423 strong pulses
of SNR ranging from 5 to 13.3 and
durations from 0.5 to 13.7 ms are detected.
As \citet{esamdin+08} noted
that five bimodal bursts were detected,
there are 27 bimodal bursts detected
with distances between two component peaks
ranging from 3 to 15 ms,
SNR from 5.5 to 9.5,
and full widths at half maximum (FWHM, W$_{50}$)
from 1.3 to 7.2 ms.
For a bimodal burst,
the SNR means the higher SNR of the two peaks
and the W$_{50}$ is calculated
from the peak of the higher SNR.

The W$_{50}$ of a burst is obtained from
\begin{equation}\label{equ_w50}
W_{50}=\sqrt{W_\text{50,obs}^2-t_\text{samp}^2-t_\text{DM}^2-t_\text{scatt}^2},
\end{equation}
in which $W_\text{50,obs}$ is
the observed FWHM,
$t_\text{samp}=0.5$ ms is the sampling interval,
$t_\text{DM}=1.109$ ms is the dispersion smearing time
across one sub-channel,
and $t_\text{scatt}=0.015$ ms is the broadening of the pulse
due to interstellar scattering.
Both $t_\text{DM}$ and $t_\text{scatt}$ are given by
\begin{equation}\label{equ_tdm}
t_\text{DM}=8.2976\times10^6\times{DM}\times{f_\text c^{-3}}\times{B}\textrm{ ms}
\end{equation}
and
\begin{equation}\label{equ_tscat}
t_\text{scatt}=(\frac{DM}{1000})^{3.5}\times(\frac{400}{f_\text c})^4\times{10^3}\textrm{ ms,}
\end{equation}
where $DM=195.7$ \dmu~is the dispersion measure,
$f_\text c=1541.25$ MHz is the central frequency of the receiver channel,
and $B=2.5$ MHz is the sub-channel bandwidth
\citep{lgs06,lk05}.

\begin{figure}
\resizebox{\hsize}{!}{\includegraphics{15953fg2.eps}}
\caption{Profiles of two typical bimodal bursts
detected from RRAT J1819$-$1458
where flux density is given in arbitrary unit.
The higher SNR of the two peaks
in each bimodal bursts
are 9.2 and 6.5
in the top and bottom panels, respectively.
Distances between the two peaks
and W$_{50}$ of peaks with the higher SNR
in each bimodal burst
are 14.5 and 4.5 ms in the top panel
and 8 and 7.2 ms in the bottom panel.}
\label{fig_bim_prof}
\end{figure}

Fig.\ref{fig_bim_prof} portrays two profiles
of typical detected bimodal bursts
from RRAT J1819$-$1458
with the distances between their two peaks
being 14.5 and 8 ms.
In Fig.\ref{fig_bim_prof},
the SNR and W$_{50}$
are 9.2 and 4.5 ms in the top panel,
and, 6.5 and 7.2 ms in the bottom panel.
The peaks of the higher SNR
appear behind
those of the lower SNR,
as shown in Fig.\ref{fig_bim_prof},
in 16 bimodal bursts,
while peaks of the lower SNR
appear behind those
of the higher SNR
in another nine bimodal bursts.
In the remaining two bimodal bursts,
the two peaks visibly
have approximately equal SNR.
There are four bimodal bursts
that are possibly ``tri-modal",
which means that one burst
has possibly three close-set peaks
with distances
between two adjacent peaks
less than 5 ms.
However,
it is difficult to distinguish
the third peak from noise fluctuations
because of the low flux density (SNR $\le3$).

\begin{figure}
\resizebox{\hsize}{!}{\includegraphics{15953fg3.eps}}
\caption{Variation of average SNR with DM.
The average SNR
that has a peak value at $DM=195.7$
\dmu~as indicated by the arrow,
is calculated
from all 423 detected bursts from RRAT J1819$-$1458
with $DM$ increasing
from 192 to 199.5 \dmu~in steps of 0.1 \dmu.}
\label{fig_snr_dm}
\end{figure}

To obtain a $DM$
closer to the intrinsic value,
with $DM$
increasing from 0 to 400
\dmu~in steps of 0.1 \dmu,
average SNR of all 423 bursts
from RRAT J1819$-$1458
are calculated
for all $DM$.
Fig.\ref{fig_snr_dm} is the graph
of average SNR versus DM
with $DM$ varying from 192 to 199.5
\dmu~and shows that
the peak SNR is
at $DM=195.7$ \dmu.
In the range of
$DM$ from 300 to 400 \dmu,
where the SNR variation behaves
like white noise,
the standard deviation in the SNR fluctuation
is 0.023 and its quintuple is 0.115.
The $DM$ uncertainty
is then limited to 0.3
\dmu~at a 5$\sigma$ confidence level.
The result $DM=195.7\pm0.3$
\dmu~is in accord with those of
\citet{mll+06} and \citet{esamdin+08}.

\begin{table}
\centering
    \caption{\label{tab_tim_para}
    Timing parameters of RRAT J1819$-$1458.}
    \begin{tabular}{lcc}
    \hline\hline
    Parameters                                      &   &Values                                 \\
    \hline
    RA (J2000)                                      &   &18:19:34.173                           \\
    Dec (J2000)                                     &   &$-$14:58:03.57                         \\
    Frequency $\nu$ (Hz)                            &   &0.234565100209(7)                      \\
    Frequency derivative $\dot{\nu}$ (Hz s$^{-1}$)  &   &$-3.09123(2)\times{10^{-14}}$          \\
    Epoch (MJD)                                     &   &54321                                  \\
    Dispersion measure $DM$ (\dmu)                  &   &195.7(3)                               \\
    Time span (MJD)                                 &   &54200.1--55299.0                       \\
    Residual rms $\sigma$ (ms)                      &   &7                                      \\
    Fundamental frequency {\sc wave\_om}            &   &0.00437                                \\
    Number of sinusoids $n_\text H$                 &   &13                                     \\
    \hline\hline
    \end{tabular}
    \tablefoot{Numbers in parentheses
    are uncertainties in the last digits,
    which are ten times the {\sc{TEMPO2}} standard errors.
    The position of J1819$-$1458
    is from \citet{rmg+2009},
    of which errors are 0.28 arcsec in both coordinates.
    With TOAs in the bottom and top residual bands
    increased and decreased by 45 ms, respectively,
    $\sigma$ is calculated
    by fitting the parameters
    using the {\sc{TEMPO2}} parameter
    \mbox{\sc{wave\_om}}
    to whiten the timing residuals.}
\end{table}

\begin{figure}
\resizebox{\hsize}{!}{\includegraphics{15953fg4.eps}}
\caption{Variation in
flux intensity with date (top)
and timing residuals (bottom)
for RRAT J1819$-$1458.
The flux intensity
is measured in an arbitrary unit
and no remarkable deviation
of flux density
is shown in the variation plot.
The timing residuals
that show a distribution of three bands
with $\sim$40 ms intervals
are calculated with the fitted parameters
listed in Table \ref{tab_tim_para}.
The rms of residuals is 17 ms and
the error bars are 10$\sigma$.
Dots with circles in the graphs
are the counterparts of bimodal bursts
and the gaps in date
are due to observation scheduling.}
\label{fig_int_res}
\end{figure}

In this work,
the flux intensity of a detected burst, $E$,
is quantified by
\begin{equation}\label{equ_int}
E=W_{50}\times{S},
\end{equation}
in which $W_{50}$ is the FWHM
and $S$ the peak flux density.
The epochs of the two glitches
associated with increases
in flux intensity
are beyond
the time range of
this observation
\citep{lmk+2009}.
Thus it is not inconsistent that
there is no burst with
a significant deviation
in flux intensity
as shown
in Fig.\ref{fig_int_res} (top).
From the figure,
there is no evidence
that the intensity of bimodal bursts
undergoes obvious deviation.

As reported by \citet{lmk+2009}
and shown in Fig.\ref{fig_int_res} (bottom),
the timing residuals of RRAT J1819$-$1458
fall into a tri-band distribution.
With {\sc TEMPO2}\footnote{http://www.atnf.csiro.au/research/pulsar/tempo2/}
in {\sc{TEMPO1}} compatibility mode
and using the same method as \citet{lmk+2009},
the parameters $\nu$ and $\dot\nu$
in Table \ref{tab_tim_para}
are obtained
by fitting the 423 TOAs
while increasing and decreasing
the TOAs
in the top and bottom bands
by 45 ms,
respectively.
Taking the two glitches
and different timing epochs into account,
the fitted values
of $\nu$ and $\dot\nu$
correspond to
those acquired by \citet{lmk+2009}.
The residuals from
fitting only $\nu$ and $\dot\nu$
have a waveform
of amplitude $\sim$30 ms
and period of $\sim$2 years.
When the residuals
are calculated
using the unmodified TOAs
and the same fitted parameters,
the residuals
in the two side bands
vary along the tracks
of invariable distances
from the center band;
the residual patterns
for the three bands
are then similar.
This shows that
the residual wave
is not caused by
random phases of the bursts
but probably
by a timing noise
of unknown origin.
The small residual rms
($\sigma=7$ ms)
in Table \ref{tab_tim_para}
is due to
the modification of TOAs
in the top and bottom bands
and using the {\sc{TEMPO2}} parameter
{\sc{wave\_om}}
to remove red noise from the residuals.
The value of {\sc{wave\_om}}
is the fundamental frequency
of the removed wave
and $n_\text H$ is
the number
of the harmonically related sinusoids
\citep[for details of the whitening method, see][]{hem2006}.
The timing residuals
presented in Fig.\ref{fig_int_res} (bottom)
and the rms $\sigma=17$ ms
are computed
from the unmodified TOAs
with parameters that take account of
the whitening parameters
in Table \ref{tab_tim_para}.
No successive bursts are
simultaneously detected
in more than one band
over intervals shorter than
the spin period
and longer
than the largest distance
of two peaks
of the bimodal bursts,
which means that
no more than one burst
is detected in one rotation cycle
at this observation sensitivity.
The middle emission area is more active
and emits about 90\% of the bursts
detected from RRAT J1819$-1458$
including the 27 bimodal ones.

\begin{figure}
\resizebox{\hsize}{!}{\includegraphics{15953fg5.eps}}
\caption{Distribution of timing residuals
of 423 detected bursts
from RRAT J1819$-$1458 (top),
and, plots of SNR (middle)
and W$_{50}$ (bottom) versus timing residual.
Circles in the two plots
are the counterparts of bimodal bursts.}
\label{fig_dist_snr_w50_res}
\end{figure}

Fig.\ref{fig_dist_snr_w50_res} (top)
is the distribution histogram
of the timing residuals
of 423 detected bursts
from RRAT J1819$-$1458,
which shows a tri-modal shape
with only seven bursts scattering
from $\sim$30 to 55 ms
in the last band.
This result agrees with
the residual distribution
reported by \citet{lmk+2009},
considering the high detection threshold
of the flux density
of the Urumqi 25-m telescope
and the low SNR
of bursts in the last band
as shown in Fig.\ref{fig_dist_snr_w50_res} (middle).
The SNR versus timing residual
is plotted in
Fig.\ref{fig_dist_snr_w50_res} (middle),
which shows that
the highest SNR is
from the middle band.
The maximum SNR
of bursts
in the last band
is $\sim$6
and the mean SNR of bursts
in the early band
is 6.5.
It is shown that
SNR of bursts
in the last band
are likely to be lower than
those in the early band.
As displayed
in the bottom panel
of Fig.\ref{fig_dist_snr_w50_res},
the average W$_{50}$ (4.0 ms)
of bursts
in the last band
is slightly larger
than that (3.1 ms)
of bursts
in the early band.
When considering
the poor quality specimen bursts
in the two residual bands,
the mean intensity (14.3 in a.u.)
of bursts in the last band
is approximately equivalent to
that (13.0)
of bursts in the early band,
which is consistent with
the result of
\citet[][Fig.2]{lmk+2009}.

\begin{figure}
\resizebox{\hsize}{!}{\includegraphics{15953fg6.eps}}
\caption{Flux intensity distribution
of bursts detected
from RRAT J1819$-$1458.
The flux intensity distribution
is generated by 266 detected bursts
with $SNR\ge6$.
The dashed curve line
signifies
that the intensity
cumulative probability distribution
is a power law.
The power-law index $\alpha=1.6\pm0.2$
is fitted from
the numbers of bursts with
intensities higher than 10.}
\label{fig_int_dist}
\end{figure}

The histogram in Fig.\ref{fig_int_dist}
is the flux intensity distribution
of 266 detected bursts with $SNR\ge6$
from RRAT J1819$-$1458.
At higher intensities,
the cumulative probability distribution
(CPD) of intensity
is probably a power law.
The power-law index $\alpha=1.6\pm0.2$
with purely formal errors
represents the best fit
for the number of bursts
of intensities higher than 10.
The fitting equation is
\begin{equation}\label{equ_cpd}
CPD=K\times{E^{-\alpha}},
\end{equation}
where $E$ is the flux intensity
in an arbitrary unit \citep{cst+1996}.
Toward both higher and lower intensities,
the deviations
from fitting curve
are possibly
due to
the small amount
of detected bursts
of low intensities
or/and
the CPD actually
not being a power law.
We infer that
it remains unclear whether
the CPD is intrinsically
a power law.

\begin{figure}
\resizebox{\hsize}{!}{\includegraphics{15953fg7.eps}}
\caption{Plot of SNR versus W$_{50}$
of 423 detected bursts from RRAT J1819$-$1458.
The plot displays that
the burst of the highest SNR (13.3)
has a medium W$_{50}$ (5.7 ms),
whereas the burst with the largest W$_{50}$ (13.7 ms)
has a comparatively low SNR (6.9).
Circled dots
are the counterparts of bimodal bursts.}
\label{fig_snr_w50}
\end{figure}

Fig.\ref{fig_snr_w50} is a plot
of SNR versus W$_{50}$
for all bursts detected
from RRAT J1819$-$1458,
which shows that W$_{50}$
widely ranges from 0.5 to 13.7 ms.
The variation in SNR
that is proportional
to the peak flux density
has no apparent relation to W$_{50}$.
The widest burst with $W_{50}=13.7$ ms
has a relatively low SNR of 6.9,
whereas the brightest burst of $SNR=13.3$
has a medium W$_{50}$ of 5.7 ms.

\begin{figure}
\resizebox{\hsize}{!}{\includegraphics{15953fg8.eps}}
\caption{Profiles of two individual pulses
from RRAT J1819$-$1458
of widely different SNR and W$_{50}$.
The two bursts are
located in the middle band
of timing residuals.
SNR and W$_{50}$
of the burst in the top panel
are 11.8 and 2.9 ms
when those of the burst
in the bottom panel
are 6.7 and 10.0 ms.
The amplitude is measured
in an arbitrary unit.}
\label{fig_nar_wid}
\end{figure}

Fig.\ref{fig_nar_wid}
portrays two typical examples of
detected individual single-peak pulses
from RRAT J1819$-$1458
located in the middle band
of timing residuals
(shown in Fig.\ref{fig_int_res})
with widely different shapes.
The spiky burst
of $W_{50}=2.9$ ms
in the top panel
has a high SNR of 11.8,
whereas the broad burst
of $W_{50}=10.0$ ms in the bottom panel
has a rather low SNR of 6.7.
As shown in Figs.\ref{fig_snr_w50}
and \ref{fig_nar_wid},
profiles of detected bursts
have various shapes with
W$_{50}$ varying broadly
without any clear relation
to the peak flux density.

\section{Discussion}\label{sec_dis}
From Figs.\ref{fig_snr_w50}
and \ref{fig_nar_wid},
the profiles
of the single bursts
of RRAT J1819$-$1458
vary from pulse to pulse.
The phenomenon
is similar to the one of
that individual pulses
of a normal pulsar
differ from each other
\citep[e.g. pulses of PSR B0943+10 as reported by][]{dr99}.
Fig.\ref{fig_dist_snr_w50_res} (middle)
shows that the average SNR
of bursts
in the last band is
lower than those
in the early band.
This is consistent with
the integrated profile
from 165 individual bursts
in Fig.3 of \citet{lmk+2009}.
It is noted that
the tri-band pattern
of timing residuals
could be interpreted
in terms of a patchy radio beam
with core and conal components
\citep{lmk+2009}.
Judging from
Fig.\ref{fig_dist_snr_w50_res} (bottom),
the widths of bursts
in the last band
are prone
to be larger than
those of bursts
in the early band.
It seems that
the pulse profiles
of bursts in
the last and early bands
are different,
while all the bursts
of the two bands
are from the ``cones".
Since the spectrum
of the ``core" component
is always steeper than
those of components
from the ``cones" \citep{lm88},
a multi-frequency
and higher sensitivity study
of bursts
from one residual band
to another
may uncover more knowledge
about the phase distribution of
individual bursts.

The power-law index
of intensity CPD
for giant pulses
from PSR B1937+21
at 1420 MHz
is $\alpha=1.8$
\citep{kt00},
and for both the giant pulses
from PSR J1824$-$2452A
at 1400 MHz
and
the Crab pulsar
at 1300 MHz
is $\alpha=1.6$
\citep{kbm+06,btk2008}.
Finding a similar value of $\alpha=1.6$
also for RRAT J1819$-$1458 at 1540 MHz
suggests that
the emission mechanism
of RRAT J1819$-$1458
is perhaps similar to
that of pulsars with giant pulses.
However,
those detected giant pulses
are from pulsars
of relatively short spin periods
measured in ms
and have short pulse durations
measured in {$\mu$}s even ns,
which are quite different
from those of RRAT J1819$-$1458.
If the small amount
of bursts of low intensities
is not caused by
observation sensitivity,
the pulse intensity distribution
of RRAT J1819$-$1458
may be similar to those of
some normal pulsars
\citep{hw1974}.

Both RRAT J1819$-$1458
and PSR B0656+14
have relatively high
magnetic field strengths
and moderate characteristic ages
\citep{lmk+2009,bt1997},
and similar X-ray emission properties
are also observed for the two neutron stars
\citep{mrg+07,dcm+05}.
The intensity CPD
and emission modulation properties
of RRAT J1819$-$1458 at $\sim$1.5 GHz
resemble those of B0656+14 at 327 MHz.
Furthermore, the latter pulsar
might have been observed as
a RRAT if it had been at greater distance
\citep{wje2010,wsr+2006}.
This indicates that
RRAT J1819$-$1458 is possibly
a normal pulsar
with pulse properties
similar to PSR B0656+14,
while its quite large distance
ensures that the former is detected
as a pulsar with sporadic pulses.
This may explain
that most known RRATs
have larger DM
than most normal pulsars,
since a large DM normally corresponds to
a large distance
that can ensure that
the modulated pulses
with low flux densities
remain undetected.
However,
there is presently
only one RRAT
with $DM>500$ \dmu,
which indicates an upper limit of DM
because an excessively large distance
would ensure that
even extremely bright pulses
of a neutron star remain invisible.

\section{Conclusion}\label{sec_con}
This paper has presented
the analysis results
of 423 detected bursts
of RRAT J1819$-$1458.
A value
of $DM=195.7\pm0.3$
\dmu~with 5$\sigma$ error
is obtained.
A simple timing result is given
and the tri-band shape
of timing residuals is confirmed.
Pulses situated
in the central timing residual band
are more complicated,
including 27 bimodal bursts,
the broadest burst,
and the brightest one.
The differences
in the average SNR
and average W$_{50}$
of bursts
in the two side residual bands
are indicated.
Profiles of
four typical individual
bursts including two bimodal bursts,
and a plot of SNR versus W$_{50}$
are presented.
A possible power-law intensity CPD
with index $\alpha=1.6\pm0.2$
is measured.

Differences
in both SNR and W$_{50}$
of single pulses
in the two side bands of timing residuals
for RRAT J1819$-$1458
are briefly discussed.
Comparisons between
the flux intensity distribution
and those of giant pulses,
and,
similarities
in the emission properties
of the RRAT
and PSR B0656+14
are also briefly presented.

\begin{acknowledgements}
The authors thank
the members of Pulsar Group
at Urumqi Observatory
for the helpful discussions.
We also thank the referees
for valuable suggestions.
This work is supported
by the National Natural Science Foundation
of China
(grant 10973026, 10903019,
10935001 and 10973002),
the Natural Science Foundation
of Xinjiang Uygur Autonomous Region
of China (grant 2009211B35),
the National Basic Research Program
of China (grant 2009CB824800)
and the Knowledge Innovation Program
of the Chinese Academy of Science
(grant KJCX2-YW-T09).
\end{acknowledgements}
\bibliographystyle{aa}

redpajama_set_name: RedPajamaArXiv


Life Skills program offers students with special needs a unique program geared towards developing functional academic skills in literacy and numeracy. Personal goals, planning and timelines are also explored to help in the planning of school experiences in preparation for adult life. Students are involved in the recycling program and monies collected are used to help subsidize field trips.
Students participate in work experience placements in the community. Placements are based on future employment possibilities and the student will learn specific skills including resume writing, interview preparation and will receive job coaching.
Some of our students are involved in community integration, volunteering at the Seniors Community Hall, shopping as part of the cooking program and using public transit.
Students receive small group and/or individual support from teachers, EAs, case managers and guidance counselors. Students who qualify also receive support and/or consultation from occupational therapist, physical therapist, speech language pathologist and Set BC consultant.


text:
Interview with Daniel Scales, Chief Brand Counsel, Linux Foundation
Linux Admin on June 3, 2021
Jason Perlow, Director of Project Insights and Editorial Content at the Linux Foundation, spoke with Daniel Scales about the importance of protecting trademarks in open source projects.
JP: It's great to have you here today, and also, welcome to the Linux Foundation. First, can you tell me a bit about yourself, where you are from, and your interests outside work?
DS: Thanks, Jason! It is great to be here. I grew up in Upstate New York, lived in Washington and London for a few years after college, and have been in Boston for the last 20+ years. Outside of work, I coach my daughter's soccer team, I like to cook and play my bass guitar, and I am really looking forward to getting back to some live music and sporting events.
JP: And from what organization are you joining us?
DS: I have been with the Boston law firm Choate, Hall & Stewart since 2011. In addition to advising The Linux Foundation and other clients on trademark matters, I helped clients with open source license questions, technology licenses, and IP-focused transactions. Before Choate, I worked as IP Counsel at Avid Technology, where I managed their trademark portfolio through a global rebranding and supported the engineering team on technology licenses.
JP: So, how did you get into Intellectual Property law?
DS: Great question. I studied economics in college and took a fantastic senior seminar on the economics of intellectual property. After graduation, I worked in the economics consulting group at Ernst & Young. A big part of my job there was determining the value of a company's intangible property, which in many cases were its brands. I went to law school intending to study trademarks and the new field of "internet law" (this term probably dates me) and started my legal career at Testa, Hurwitz & Thibeault, which had a cutting-edge trademark and open source group.
JP: We typically think of IP and Trademark law as it applies to consumer products and commercial entities. What is the difference between those and when open source projects and organizations use brands?
DS: On one level, there really isn't a difference. A trademark signifies the unique source of a good or service. Trademarks help consumers, developers, and users distinguish various offerings, and they communicate the specific source and quality of those offerings. Software developers and users need to understand what code they have and where it came from. Trademarks help communicate that information. Of course, the specific issues that every brand and brand owner faces and how they address them are different, but many of the core principles are the same.
JP: What are some of the trademark issues you've seen come up in open source communities?
DS: While it happens in every industry, I see many "helpful" people apply to register projects' trademarks when they are not the rightful owner. Sometimes they have good intentions, sometimes not, but it can be a lot of work to sort it out either way. I've also had the opportunity to work with many different people and companies on project branding. It is amazing how many different philosophies there are regarding branding, even within the software industry. Much of what we do is to bring these folks together to determine the best approach for the specific project. I also spend a lot of time debating the scope of trademark rights with opposing counsel, but that isn't really unique to open source: one lawyer tried to convince me that his client had the exclusive right to use a picture of a hop flower on a beer label.
Other common issues are helping companies register a mark for their company or product and then used the same mark for an open source project. The neutrality of those situations is imbalanced, and the Linux Foundation has worked with organizations making this transition. Sometimes it involves rebranding the open source project, and we assist in finding and clearing a new name for the community to use independent of the company that started it.
JP: Why is the Linux Foundation a good place for open source projects to protect their brands?
DS: We have worked with many open source projects on their trademarks, and we learn something with every new experience. We can help them name the project at the beginning, take steps to protect their trademarks across the globe, and show them how trademarks can be a tool to build their communities and increase participation and adoption. We also recognize the importance of our neutral position in the industries we serve and how that is fundamental to open governance.
Also Read: Open Source Communities and Trademarks: A Reprise
JP: Trademark conformance can also protect a project from technical drift. How can a trademark conformance program be used to encourage conformance with a project's code base or interfaces?
DS: Great point. As in most areas of trademarks, clarity and consistency are key. Trademarks used in a conformance program can be a great tool to communicate quickly and accurately to the target community. Projects can develop specific and transparent criteria so that users understand exactly what the conformance trademark symbolizes. This can be much more effective and efficient for projects and users alike than everyone deciding for themselves what a term like "compatible" might mean.
Also Read: Driving Compatibility with Code and Specifications through Conformance Trademark Programs
JP: Do projects at the Linux Foundation give up all control of their trademark? How do you decide what enforcement to pursue or not pursue?
DS: On the contrary — we work very closely with project leadership throughout the lifecycle of their trademarks. This includes trademark enforcement. Typically, the first step is to figure out whether the situation requires enforcement (in the traditional legal sense) or if it is simply a matter of educating another party. More often than not, we can reach out to the other party, discuss our project and our trademarks, discuss our concerns, and work out a solution that works for everyone and strengthens our brands. But like any brand owner, we do sometimes have to take other action to protect our projects' trademarks, and we work closely with our projects in those situations, too.
JP: Thanks, Daniel. It's been great talking to you today!
Linux Mint 6 "Felicia" x64 RC1 released!
Weekly Newsletter – Issue 57
Daryna KDE CE B44
Rancher – Your Private Container Service : Run Containers in Production – Install Rancher on CentOS 7 / Ubuntu 16.04
Previous: Previous post: Visual Studio Code at Microsoft Build 2021
Next: Next post: The Zephyr Project Celebrates 5th Anniversary with new members and inaugural Zephyr Developer Summit on June 8-10
How to Disable Inspect Element in WordPress

redpajama_set_name: RedPajamaCommonCrawl


3 wheels have steel inserts inside lug nuts holes (professionaly done) and all four showing 5×112 mercedes bolt pattern.One wheel is without inserts. Please check the pictures with wheel bolt pattern tool for details.
Please check those pictures carefully for condition.
Those wheels has been sitting in my warehouse for 20 years and they can be dusty and have some imperfections and scratches.
When I remove them from boxes two of those have brabus stickers on the face,but not sure why. No center caps included.Selling as used. Please check the offset and wheels size to be sure those wheels fit your car.
Style 38 3 spoke wheels with all the nostalgia of the 90s!
DP Motorsport are known for their high end Porsche tuning equipment.
Same Wear, please review all photos before biding.
Four hubcaps with 16.25" outer diameter (for 15" wheels) to fit them.
These provide a classic look, yet still are able to use higher speed 15" tires (as opposed to 14"). They are currently equipped with 4 cracked Michelin 205/65/15 tires and one spare tat is in better shape.
The pricing is for local pickup, but I am willing to ship the wheels and hubcaps at the buyer's expense.
If desired, the tires can be removed and disposed of for an additional $50 after the sale.
These wheels and hubcaps took a long time to find, purchase, deliver from Germany, and finally be ready to sell.
Tagged 600, 911, 993, AMG, BMW, Brabus, Bundts, Dinan, DP Mptorsports, Hubcaps, Mercedes Benz, Monoblocks, Porsche, Speedline, Style 38, targa, W100.
I'll take the steelies with the hubcaps.


Taxi Mauritius / Destination Soleil based in Baie du Tombeau, Mauritius. We have riched experience in organizing excursions throughout the island. Since more than a decade, we have pioneered this organization since its very inception.
In our service, we privilege the quality instead of the quantity, because our main priority is the satisfaction of client. We provide comfortable vehicles on competitive rates. We are not only specialized in offering visits of different sites and views but also get you to discover the different cultures and foods available in the beautiful island of Mauritius.
We are well equipped to handle all types of holidays. Over the years, this team has grown. Today, Taxi Mauritius / Destination Soleil online operates as tour operator for thousands visitors from all over the world.
Our management team is committed to provide personalized services to all the clients with total professionalism.


text:
Чо́ртова Ске́ля — лісовий заказник місцевого значення в Україні. Розташований у межах Личаківського району Львова, на південь від села Лисиничі і на захід від м. Винники.

Площа природоохоронної території 353 га. Створений 1984 року. Перебуває у підпорядкуванні ДП «Львівський лісгосп», Винниківське лісництво.

Основними завданнями заказника є збереження цінних букових, дубових, граба і буково-соснових лісів з мальовничими ландшафтами та скелями.

Заказник розташований у межах Львівського плато, у Винниківському лісопарку, в районі пам'ятки природи — Чотові скелі, які є ерозійними останцями верхньотортонських пісковиків з мальовничою вершиною. Вся територія лісового масиву характеризується мальовничими ландшафтами; тут також виділені генетичні резервати букових лісів. Територія розташована в лісопарковій частині зеленої зони Львова.

Фотогалерея

Джерела
 Лісовий заказник «Чортова Скеля»

Лісові заказники Львівської області
Винники
Природоохоронні об'єкти, засновані 1984

redpajama_set_name: RedPajamaWikipedia


Fran Brown owned a young pony, Titch. She was training him towards her dream of one day becoming a top class show jumper. In return for lessons she does stable work for Selina Pratt-Smythe.
Hilda Newman had discovered a love of horse riding, which her mother strongly objected to, because Hilda was blind and she was afraid she would get hurt. People were also against Hilda's horse, Buccaneer, who worked well with Hilda but was good tempered around others due to mistreatment in the past.
Diana Evans has been tricked into going to the small country of Lituanna with her pony, Bronwen, bought by King Remo, who wants Diane to teach his daughter, Zahra, to ride. Diana discovers that the people of Lituanna live in fear of their High Priest, whose temple she accidentally comes upon. Puzzled as to why she has been brought to Lituanna. Diana asks the crippled King Remo for an explanation.
Dangerous Days for…Diana Evans – Judy: circa #144 (13 October 1962) – #152?
Bonny and Cly, the big Clydsdale horse, had a spell put on them by Whirlin the Wizard. They were banished until they found the Golden Gooseberry. As part of the spell, Bonny could understand what Cly was saying.
During the eighteenth century, times were hard for Cora Thatcher's parents and they were forced to sell their fine horse, Starlight. Charles Beaufort, a wealthy landowner, bought the horse for his spoilt daughter, Clarissa. Because no-one else could handle the horse, except Cora, she was "bought" too. Although the valuable horse was well fed and tended, life was grim for Cora.
Netta's family can't afford to buy her a horse, so Netta works for a mean horse dealer, Mr Mundy, who allows her to ride any unsound horses.
No Horse For Netta– Bunty: circa 675 (19 Dec 1970) – ?
Two cousins who dislike each other have to share a pony they inherited from their grandfather.


text:
Intra-state bus services resume in Punjab
Public bus services resumed in Punjab on Wednesday almost two months after their suspension in the wake of the COVID-19 outbreak. Buses of the state-owned Punjab Roadways and Pepsu Road Transport Corporation (PRTC) plied on select routes in non-containment zones within the state, officials said.
As per news report of PTI, Punjab Transport Minister Razia Sultana had on May 18 announced resumption of point-to-point bus services between major cities and district headquarters from May 20 with 50 per cent occupancy.The state government has said inter-state bus services will not resume till May 31.
Source -PTI


text:
Banger Music
Bangin Rumours
Celebrate Curtis Mayfield's Birthday with This Vintage 1972 Concert
Curtis Mayfield, who would have turned 78 today, is best known for his smooth, soulful pipes, but he was also one of music's most prominent social commentators. His success with The Impressions during the Civil Rights movement and later as a solo artist left a huge mark, not just on the African American community, but well beyond. In 1972, he recorded the soundtrack to the blaxploitation crime drama Super Fly, which addressed issues like poverty and drug abuse and became one of his most beloved albums.
On November 2, 1972, Mayfield performed three songs from Super Fly at Hofstra University in Hempstead, N.Y. On Super Fly, Mayfield skillfully melds intricate psych-funk with slick soul, and this performance captures Mayfield's swift guitar improvisation and his gentle yet transcendent vocals.
Read: An Exclusive Excerpt from the Curtis Mayfield Biography, Traveling Soul
Watch Curtis Mayfield's full performance from 1972 below.
Nation of Language Share Video for "On Division St"
Angelo De Augustine Shares New Song Featuring Sufjan Stevens, "Santa Barbara"
Bartees Strange Announces Debut Album 'Live Forever,' Shares New Single
Hear Miles Davis Soar in a Career-High Moment on This Day in 1971
Hear Tears for Fears Perform Selections from Songs From The Big Chair in 1985
Billie Eilish & Rosalía Join Forces on "Lo Vas A Olvidar"
Weezer Share Video for Lead Single "All My Favorite Songs"
Watch Bruce Springsteen, Katy Perry, New Radicals and More Perform at President Biden's Inauguration
Dawn Richard Signs to Merge, Will Release New Album in 2021
Arlo Parks Announces New Variety Special with Glass Animals, Romy of The xx, Dave Okumu


text:
State Terror
1 March 2022 22 December 2022 4WardEverUK
The Ukrainian refugee crisis has already begun (the UN reports)
source: Vox News
The United Nations has estimated that about 100,000 Ukrainians have already been displaced as a result of the Russian invasion, and that number could ultimately grow to 1 to 5 million. The international community is making preparations to meet their humanitarian needs — though perhaps not quickly enough.
Just hours after Russia's assault began on Thursday morning, there were massive traffic jams, sold-out train tickets, and long lines at ATMs in Kyiv as people tried to flee with little clue as to how long they might be gone or if they'll return.
21 January 2022 22 December 2022 4WardEverUK
The dark truth about closing the Guantánamo Bay prison
originally by: Alternet
It's now more than 20 years later and that American offshore symbol of mistreatment and injustice, the prison at Guantánamo Bay, Cuba, is still open. In fact, as 2021 ended, New York Times reporter Carol Rosenberg, who has covered that notorious prison complex since its first day, reported on the Pentagon's plans to build a brand-new prefab courthouse at that naval base.
It's intended to serve as a second, even more secret facility for holding the four remaining trials of war-on-terror detainees and is scheduled to be ready "sometime in 2023."
Celia Stubbs, partner of Blair Peach, to appear at Undercover Inquiry
source: Big Issue North
Celia Stubbs, whose partner Blair Peach was killed by police 42 years ago, hopes her appearance at the Undercover Policing Inquiry will help her discover why she was spied on for decades.
Stubbs, 81, and still active politically by supporting refugees and asylum seekers, is among thousands of political activists that members of the London Metropolitan Police's Special Demonstration Squad (SDS) highlighted for attention from 1968 onwards. Targets included women, with whom officers sometimes had relationships and children.


Proctor2Me: Is it really you?
Dreaming of a job, or create the job of your dreams?
Innovation comes from small companies, most of the time. Small companies also generate most of the employment. So it is important to foster young startups and let them grow easily….


In this episode of TWIST Conversations I chat with Saif Altalib of AT&T University. In this discussion, we explore a Performance Support solution built by AT&T University that combines Social, Mobile, and Cloud-based elements to provide the support needed by workers when they need it, and where they need it.
Saif explains the challenges sales people were encountering, and how this unique Performance Support solution was developed to provide workers with the ongoing support they needed.


Having a brand new, clean car is great, but the synthetic "new car scent" can get irritating after a few days. Not only is this scent annoying, it can also be harmful to your health as it usually is a byproduct of the noxious car polish and plastic covers that make your car look so new and shiny. Eliminate this smell by first removing all the plastic covers on the interior of your car and leaving the windows open to air out your car. Then use absorbent materials like baking soda to soak up the smell, as well as air fresheners and sprays to give your car a new, pleasant scent.
Remove interior plastic coverings. One of the main culprits of the chemically new car scent are the plastic coverings that keep the interior pristine. Remove all the plastic coverings from the inside of your car, including the seat covers, the plastic around the dashboard and cup holders, and the lining on the interior doors of the car.
Leave the windows open. If weather permits, leave the windows open in your car as you are driving around, and consider leaving them open overnight to let the chemical scent escape and let the fresh air come in. Try to keep the windows open when you can as long as you still smell the new car scent.
Park your car outside if possible. Even if you don't feel safe leaving your car's windows open overnight, try to park your car outside when you're not driving it. Since some of the odor comes from the exterior car polish and window cleaner, leaving your car out in open air still helps to air out the scent of the exterior.
Leave your car out in the hot sun. Though it's difficult to say why it is effective, leaving your car in the hot sun with the windows cracked is an effective way of "baking" away the stubborn new car scent. Try to leave the car in the sun for at least two hours to lessen the car smell.
Leave the heat on for several hours. If it's a gloomy day or the sun isn't out in your area, another way to bake out the smell of your car is to close the windows and keep the heat on high for several hours. After two to three hours, turn the heat off and open the windows to let the car air out.
Make sure you do this outside, as doing it in a sealed garage will cause carbon monoxide to build up in the air.
Keep the vents in your car running fresh air. Something you want to avoid when you're driving is to re-circulate the chemical-filled air inside your car. When you're in your car, run the vents on high under the "fresh air" setting rather than the "recirculate" setting to bring air from outside into your car.
Use baking soda to soak up the scent. To absorb the odor of the car's interior, place a few scoops of baking soda in an uncovered container like a bowl or Tupperware container. Place the container in a secure location of your car where it won't get knocked over and let the baking soda absorb the noxious odor of the car for about a day.
If the smell still persists after a day, empty out and replace the baking soda. You can also try other absorbent substances that may work better at soaking up the smell.
Soak up the scent with vinegar. White vinegar is another absorbing agent that is effective at combating strong smells. If using baking soda didn't work, add two parts of vinegar to one part water in a small container like a jar with a few holes poked in the top of the lid. Place the jar or container in a secure place in your car, then leave it there for about a day so that the vinegar can soak up and mask the odor.
Place barbecue charcoal under the seats. Another unlikely but effective absorber of scents is barbecue charcoal. To use, place a couple pieces of charcoal on top of paper towels and put them under the driver's and passenger's seats for a couple of days or until the odor is gone.
Clean the interior of your car. Since the new car scent is caused in part by the new plastic of the interior of the car, cleaning and wiping interior plastic surfaces can help to remove the odor. Use a gentle cleanser and a microfiber cloth to clean any plastic interior surfaces such as the door or the steering wheel. After using the cleanser, wipe surfaces with a damp cloth to make sure the cleanser is completely removed from the plastic and doesn't leave streaks.
Get your car detailed. Another way to clean away the new car smell smell is to get your seats and carpet shampooed at a detailing shop. Seats and carpeting are often made of absorbent material, which may absorb and trap the new car odor. Even though detailing is usually done to remove dirt and dust, it can work to remove bad odors as well.
You can also do this yourself by buying products made specifically for the materials in your car interior and following the instructions on the label.
Getting this procedure done is effective but can be quite expensive, so you may want to try other methods and use this as a last resort.
Steam clean your seats. An alternative to shampooing your car seats is to steam clean them. Steam cleaners shoot steam deep into upholstery to break down and eliminate bad scents. You can buy or rent steam cleaners in many home improvement stores, but be careful to follow the instructions on the label as steam can burn if used improperly.
Use air fresheners. If you have tried airing out and cleaning your new car, you should have been successful in eliminating most of the odor. If you have a small amount of odor left, you can easily mask it by hanging an air freshener from your rearview mirror or spraying around a deodorizing spray. Use your favorite scent and make sure the freshener is near the driver's side of the car so that you can smell it.
Buy an industrial strength odor eliminator. If you want to do more than just mask the smell, consider buying an industrial strength odor eliminator. These can be found at automotive stores and are formulated specifically for neutralizing bad car odors.
Use other strong scents to mask the smell. There are certain smells that are extremely potent and have a reputation for lingering. The smell of fast food or popcorn for instance can often linger long after the food is eaten. Perfumes and colognes are also formulated to have a lasting scent. Introduce a new scent into your car that you know will be able to last and mask the new car smell until it is gone.
Only do this if you like the smell that you are introducing, or else you could have an even bigger problem on your hands!
Try to absorb and air out the smell before you resort to masking it.
Sometimes your car just needs some time to get rid of the smell. Do your best to remove the smell, but be patient if you can still catch a faint whiff of it. If the smell lingers for more than a few weeks, try out more ways of removing it or consult a car detailer.
Only use cleaners formulated for the materials your car interior is made of, or you could risk doing damage to your car.
Be extremely careful and follow the instructions on the package if you are using a steam cleaner.
Thanks to all authors for creating a page that has been read 24,214 times.


I watched The Polar Express for the first time last night and was very impressed with the realistic rendering of the 3D human characters in it. I felt a little let down by the quality of the characters' hair though. After all, this was the biggest budget animated film of all time so you'd think they could afford to make the hair-dos a little more lifelike. It's not like the technology doesn't exist for modeling hair either, and there are plenty of ways to add a realistic barnet to a 3D model on your home computer.
The latest version of 3ds Max added a whole new Hair and Fur system enabling you to create and manipulate hair directly in the viewports using its selection and styling tool. Hair can be copied and pasted from one object to another, and artists can derive hair from splines and convert it to splines or meshes. Notably, any source object can now been instanced as hair strands, allowing you to accurately mimic a person's real style.
If you're a LightWave user then you'll no doubt have a tougher time of rendering hair because the app doesn't have the same fibre system as its rival. However, there are some decent plug-ins available that can help you dress the head of your models. Sasquatch is one of the most popular, integrating its own photoreal hair rendering engine into LightWave. Over 50 texturable controls give you precise control over the style, color, and shading of fur and hair. You could also try Fiber Factory, a cheaper solution, which creates polygonal fibre models such as fat hair, feathers and triangle strips.


Doherty & Clark were founded in 1972, with 36 years experience in wheel and tyre service. The Business is owned by brothers Brent and Justin Doherty, with 2 great locations this family run business offers great customer service and a friendly atmosphere.
Doherty & Clark specialise in on-site service, wheel alignments and offer a car pick up and delivery service.
We specialise in truck and bus tyres, so you don't have to look around anymore for those hard to find tyres.
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With state of the art equipment we can balance and align your wheels and tyres, prolonging the life and wear.
We understand that you work, that you have an important life, and for this reason we will pick up your vehicle and deliver it back to you, ensuring it doesn't disrupt your day.


Two major open source IoT frameworks — the OCF's "IoTivity" and the AllSeen Alliance's "AllJoyn" — are moving toward interoperability, and possibly, a merger.
Richmond also seemed open to a merger, although he framed this as a more challenging goal. "The political part of this is going to be with us even if we make the technical problem less severe," he said.
The launch of the OCF in February was seen as a major victory for IoTivity in its competition with AllSeen and other IoT groups. IoTivity emerged in July, 2014, from the Open Interconnect Consortium (OIC), with members including Intel, Atmel, Dell, and Samsung. OIC and IoTivity arrived seven months after The Linux Foundation joined with Qualcomm, Haier, LG, Panasonic, Sharp, Cisco, and others to found the AllSeen Alliance, built around Qualcomm's AllJoyn framework. Shortly before OIC was formed, Microsoft joined AllSeen.
In November of 2015, OIC acquired the assets of the Universal Plug and Play (UPnP) Forum, and in February of this year, OIC morphed into OCF. The transition was notable not only for the fact that OCF would be hosted by The Linux Foundation, which already sponsored AllSeen, but that Qualcomm, Microsoft, and Electrolux had joined the group.
The three companies remain AllSeen members, but the cross-pollination increased the potential for a merger between the groups — or if not, perhaps the rapid decline of AllSeen. Behind the scenes, a big change from OIC to OCF is the emergence of a new plan for adjudicating intellectual property claims within an open source framework, as detailed in this February VDC Research report.
In Richmond's view, IoTivity and AllSeen are both well-suited to bring order to the fractured IoT world because they're horizontal, mostly middleware-oriented frameworks. Both are agnostic when it comes to OSes on the one hand or wireless standards on the other.
At the end of the keynote, Richmond flashed a slide of a wedding invitation and then invited to the stage Greg Burns, who was the central creator of AllJoyn when he worked at the Qualcomm Innovation Center (QIC). Burns, who is now Chief IoT Software Technologist at Intel, has been one of the most active proponents of a merger.
"That's my hope, too," added Richmond.
In another ELC presentation [PDF], called "AllSeen Alliance, AllJoyn and OCF, IoTivity — Will We Find One Common Language for Open IoT?," Affinegy CTO Art Lancaster seemed to agree that a high degree of interoperability was possible — but not at the expense of killing off AllSeen. Affinegy, which has developed the "Chariot" IoT stack, has been a major cheerleader for AllSeen, and Lancaster emphasized that AllSeen has a big lead in certifications compared to Iotivity.
Both Richmond and Lancaster made it clear that there are many dozens of other overlapping IoT interoperability efforts that must also be considered in developing a universal standard. At ELC, Intel's Bruce Beare gave a presentation on one of them, Google's open source Weave framework. Meanwhile, Samsung's Phil Coval delivered a presentation on integrating IoTivity with Tizen, which Samsung is increasingly aiming at IoT.
Watch all 150+ session videos from Embedded Linux Conference + OpenIoT Summit North America here.


I did received this from the publishing company in exchange for an honest review.
I DNF'd this half way through. I loved the story set in 1982 but the current day, It just drug on. I finally just set it aside but never picked it up again. It never intriqued me enough to finish. The current day bored me and I could not get into it.
But we in 1982 we start with a young girl being hung from a tree and being stoned to death by 2 young boys. It was very detailed on the explicit scenes where you can imagine what the girl looked like and that story kept me wanting to know more but like I said, current day where the children where all older, was just boring and I am sure toward the end of the book the story may have come together but I did not want to put myself in a reading slump trying to get there.
Some may find they really enjoyed this but I just could not push through. I did give It 3 stars because I truly enjoyed the 1982 story.


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Xreferat.com » Топики по английскому языку » Stratford-upon-Avon
Stratford-upon-Avon lies at the very heart of England. It attracts people not only by its history and connection with William Shakespeare, but also by its wonderful nature and typical English character.
Stratford stands on the river Avon and is one of the oldest market towns. It has still preserved its own character and atmosphere, as you will not see modern buildings there. The houses are small and lot of them are very old. Some of them date back to Shakespeare's time. Here you can visit Shakespeare's birthplace (it is a museum now), Anna Hathaway's cottage (the early home of Shakespeare's wife), the foundations of the New Place, where Shakespeare lived when he retired and died in 1616 (now there is only a wonderful garden on the place of the house). Just round the corner there is Grammar school that Shakespeare used to attend.
Here in Stratford there is Holy Trinity Church where William Shakespeare was buries. Thousands of people from all parts of England and foreign visitors come here on Shakespeare's birthday (23rd April) to pay tribute to the great poet. Among other sights connected with the name of Shakespeare there is an interesting monument with the statue of the great poet on top and with characters from his plays round it.
And, of course, you should visit the Royal Shakespeare Theatre, a red-brick building standing on the banks of the Avon. It was opened on 1932 as a living memorial to the poet's work.
The Royal Shakespeare Company, which is one of the best known and largest theatre companies in the world, regularly performs here and in the Barbican Centre in London.
William Shakespeare was born on the 23rd of April 1564 in Stratford-upon-Avon. Father of William Shakespeare, John Shakespeare, was a merchant. He sold leather gloves and was rather successful. He was even going to be become the Head of Stratford-upon-Avon.
W. Shakespeare W. Shakespeare's father, John Shakespeare was … a)	a teacher b) a glove-maker	c) a doctor. They lived in … a) Hanley Street	b) Oxford Street	c) Wood Street
Театр.
History of creation Westminster Abbey, its restoration in the Gothic style in honor of Edward the Confessor. Erection under the direction by Sir Christopher Wren and Nicholas Hawksmoor two western towers as an early example of Gothic Revival design.
British theatres
Британские театры.
Personality of Hamlet
Among Shakespeare's many great works, Hamlet probably is the greatest. The whole play is about power and authority. The king of Denmark was murdered by his brother Claudius, who married his wife Gertrude, and became a king of Denmark. Hamlet was the son of murdered king, who was getting his ed...
Places to Visit in England
Достопримечательности Великобритании.
Жизнь и творчество Шекспира
Created three since superfluous century back tragedies, historical chronicles and the Shakespeare's comedies live till now, excite and shake imagination of the spectators. The best theatres of the world and the outstanding actors until now consider for themselves as examination and happiness to put ...
Шекспир english
Краткая биография Уильяма Шекспира. Классификация его произведений.
Theatre in Great Britain
Театр в Великобритании.
London - capital of England, its geographical position, the population and history. London and its sights, outstanding monuments: The Tower of London. St Pauls Cathedral. Trafalgar Square. The river Thames as city centre, history of its bridges.
William Shakespeare english
Биография и творчество William Shakespeare.
A museum
Музей.
Вильям Шекспир.
Изучение иностранных языков /english/
Происхождение английского языка. Влияние Вильяма Шекспира на английскую речь. Английский - международный язык. Слэнг.
Theatre, Music and Cinema
Театр, музыка и кино.
Visiting Theatres
Посещение театров.
The Life and Times of Shakespeare
Literary heritage of the great English dramatist of England W. Shakespeare. Shakespeare's career unfolded during the monarchy of Elizabeth I, the Great Virgin Queen from whom the historical period of the Bard's life takes its name as the Elizabethan Age.
Искусство /english/
Рассмотрены такие виды искусства, как: художество, музыка, литература, театр. Великий писатель - Вильям Шекспир. О музыке 60-х годов. Знаменитые художники.
London is one of the largest cities in the world. More then 10mln people live in London and its suburbs. London is a city of striking contrasts. Here one can come across the past and the present, the old and the modern, live side by side in mutual tolerance and respect.


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Know Your Employee (KYE)
Q5id Guardian
About Q5id
A Beginner's Guide to Identity and Access Management
By Tulay BanJanuary 16, 2023No Comments
As more information is published online, the higher the risk of cybercrime becomes. Online security is increasingly being reinforced, especially since cybercriminals are finding elaborate ways to steal data and commit fraud.
In response, institutions are continuously looking for ways to thwart these bad actors before they successfully commit a felony. Due to increased risks, organizations prioritize stricter security protocols connected to customer identity and access management.
What is Identity and Access Management (IAM)?
An IAM system gives organizations control over who can access their resources and sensitive information. This framework deals with business processes, policies, and technologies. With this system in place, IT administrators can restrict user access to sensitive data within their organizations.
Companies can lower the risk of data breaches and cybersecurity issues by providing centralized control to authorize resource access. Identity and access management aids by following guidelines and complying with regulations. Enterprises should consider implementing IAM to strengthen their cybersecurity posture.
What is the Difference Between Identity and Access?
The subject of identity management pertains to user authentication. It integrates digital features and database information to create a distinct identity for each user that may be utilized as a source of truth during authentication.
Finding out who is attempting to access an account or a database is the first step toward robust security.
Each request must go through a process, with the requestor's identity verified and authenticated. Using biometrics in identity management helps prevent another party from copying user information.
The main goal of access management is to control the privileges of individuals who use a given system. The system manages the access portals through login pages and protocols and helps ensure that a specific user requesting access has the proper clearance.
Access management establishes a user's identification and characteristics to grant authorization.
Although it does not manage the data, it evaluates the identity.
Components of an Identity and Access Management Framework
The three primary functions of IAM systems are identification, authentication, and authorization—only the right people can use computers, hardware, software, or any other IT resources in a given system. They are also the only ones allowed to carry out particular duties. Among the essential elements of an IAM framework include the following.
1. Database management
Managing an identity database is the initial stage in implementing IAM. Firms must record a user's distinct identity to keep track of their behavior in the system. This collective database allows organizations to record transactions, data, and accounts, making it easier to see who's part of the system and who isn't. Additionally, it's necessary to manage the user's location and every device they use to log into.
2. User identification, verification, and authentication
Identity fraud is rampant today. According to the Identity Fraud Report 2022, the average identity fraud rate between October 1, 2020, and 2021 was 5.9%, up from an average of 4.1% in 2019. Since fraudsters are becoming more inventive with their schemes, identification, verification, and authentication to recognize a user as an organization member is now more crucial.
Passwords, tokens, OTPs, and biometrics are just a few of the methods used for authentication. Effective IAM uses a multi-factor authentication system that includes several different techniques. Users can feel secure dealing with an organization when they exhaust their efforts in ensuring secure transactions.
3. Compliance auditing
IAM elements that are important for compliance must regularly be checked to see how they tie into a company's compliance plan of protecting the confidentiality, integrity, availability, and privacy of information. Proper compliance allows clients to do business with organizations in complete confidence while the company builds a solid reputation as a trusted partner.
4. Provisioning/Deprovisioning
IAM streamlines the onboarding and offboarding of clients by using procedures that restrict or permit access depending on the clearance and authorization of the person. Creating, updating, and deleting user accounts in several applications and systems is known as user provisioning and deprovisioning.
This access control procedure occasionally includes related data, such as group memberships, user privileges, and even the groups themselves.
5. File permissions
Permissions must be modified for each user after the roles are established and access to the files is granted. The user's process will determine whether the permissions given to them are to edit, view, comment, or share. For instance, clients may only be granted view access, whereas employees edit access.
Another crucial element of IAM is reporting. The user's login history, rights, and user activity, among other things, may be included in the report. To discover any strange behavior, organizations must conduct a thorough audit. Some IAM tools track how users interact with your IT infrastructure.
IT staff can immediately spot unusual activity and prevent breaches by monitoring user behavior and activity. Logs show the tools your employees use and how they use them. This information may be used more precisely to fine-tune attribute or role-based access control policies and restrict unauthorized access.
Benefits of Identity and Access Management
According to the Aite-Novarica Group, 47% of Americans experienced financial identity theft in 2020. This report solidified that fraudulent crimes against identities are still on the rise, and organizations are left to fend off cybercriminals by themselves without proper protection.
While there are numerous security tactics your firm may use to stop cyberattacks and secure your company's data, here are some of the major advantages of IAM that make it an intelligent choice for prominent enterprises.
1. Reduced chances of data breaches
IAM systems assist businesses in lowering the risk of data breaches by limiting users' access to critical information. Attribute-based access control is governed by strict standards that ensure all rights granted to people and services are correctly validated, authorized, and audited.
2. Reduced IT costs
IAM systems increase the productivity of your IT team by automating manual processes for job modifications, employee onboarding, offboarding, and user enrollment. In addition, single sign-on solutions decrease help-desk calls and service requests, freeing up IT resources.
3. Centralized access control
IAM allows organizations to manage people, devices, authentication methods, roles, permissions, and locations using a centralized platform. This makes it convenient for your security staff to monitor every user's behavior efficiently.
4. Enhanced security
Even if an unauthorized person breaches the perimeter, the IAM methods reinforce the system's security, preventing access to sensitive data. This helps thwart fraudulent plans and keeps proprietary information restricted.
5. Maintained or increased compliance
IAM systems can assist firms in adhering to legal compliance standards. Organizations frequently use IAM tools to automate compliance-related procedures, making it simpler to satisfy and confirm compliance with relevant standards. In addition to the losses brought on by a violation, failing to comply with these obligations might have severe repercussions.
IAM systems allow businesses to respond to audits and show that any necessary data may be available immediately. Additionally, monitoring and tracking activities enable them to improve compliance and security postures.
6. Automated system
Automation tools enable enterprises to function more effectively by saving time, effort, and money than manually managing network access. Furthermore, IAM ensures that the appropriate worker has access to the proper documents and each employee follows a system process. IAM systems can grant or prohibit access so that employees don't unintentionally delete or access them, preventing considerable losses.
7. Enforced security regulations
An IAM framework simplifies how security personnel manage and enforce user access authentication policies. This ensures that privileges are appropriately assigned, users who leave the system have their credentials revoked, and access to sensitive data is directly related to job function and not granted without the necessary clearance.
Reinforcing Your Business' Security
With the world transitioning to the digital space, it's vital for enterprises to remember that to build relationships and rapport with clients, they must first establish trust. Don't wait for a breach to happen before doing anything about it. Security protocols such as identity and access management solutions should be implemented before running a business.
Security plays a big part in organizations that handle client accounts, data, and information. Furthermore, compliance takes a lot of time and money. The best way to safeguard data and protect your reputation is to implore the help of professionals who offer expert services backed by years of experience and the latest technology in data security.
Organizations need scalable security and compliance systems to boost productivity and support new technologies, tools, and platforms for remote and hybrid workforces as they evolve. Don't be the last to protect, grow, and innovate your business. Team up with the expert from Q5id and get the latest solutions in cybersecurity for your organization.
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Players must have the following paperwork in order to start practice on the 19th.
Physical Form--see the Coach's Corner for more information about physicals.
Emergency Card--one emergency card must be filled out completely and submitted to the coaching staff.
Baseball Policies and Contract--each player and his parent must read and sign the Baseball policies and contract and submit to his head coach. Please read the contract and rules carefully to avoid any confusion.
Athletic Eligibiliy--athletic eligibility will be checked for all players with the exception of incoming freshmen.