text:
\section{

\section{Introduction}

Binaries in stellar associations are unique tools, as far as the determination of their astrophysical parameters is concerned. In an effort for identifying eclipsing binary members of stellar associations, several known binary systems in the direction of selected associations have been observed and analyzed with modern analysis techniques \citep[see][]{bakis11, bakis14}. Indeed, observational studies have shown that the multiplicity rate in OB associations is high \citep{bakis15}, as predicted by theoretical studies \citep[see for instance][]{kouwenhoven07}.

The binary star MQ~Cen and the stellar association Crux~OB1 subjected to the present study are located within the borders of the constellation Centaurus. The region partitioned by \citet{humphreys} has been presented in Fig.~1 with the open clusters in the same direction, whose distances and ages range between 780-3400\,pc and 4.3\,Myr - 1\,Gyr \citep{kharchenko05}, respectively. The mean distance of Crux~OB1 is estimated by \citet{kaltcheva} as 2700~pc. The historical studies in the region are very well summarized by \citet{tovmassian} who remarked several B associations up to the distances of 850 pc and several O associations between 1200~pc and 4000~pc for the same direction.

\begin{figure*}
	\begin{center}
		\resizebox{100mm}{!}{\includegraphics{fig1.eps}}
		\vspace{.2cm}
		\caption{Crux~OB1 region partitioned by \citet{humphreys}
			between Galactic longitudes \textit{l}=293$^{\circ}$.5 to 295$^{\circ}$.9 and between Galactic latitudes \textit{b}=--2$^{\circ}$.4 to +0$^{\circ}$.1.}\label{fig1}
	\end{center}
\end{figure*}

Having a secondary component at the turn-off point of the main-sequence, MQ~Cen is an interesting eclipsing binary located in the direction of the Crux~OB1 association. The photometric variations of MQ Cen (HD 309074, $V$=10.2\,mag, $\alpha_{2000}=11^{\rm h}\,44^{\rm m}\,16^{\rm s}$, $\delta_{2000}=-61^{\circ}\,42'\,59''$) were discovered by \citet{guthnick} on photographic plates with an amplitude of 0.4\,mag. Since its discovery, there have been a few studies where the times of minimum light of the primary eclipses have been presented \citep[e.g.,][]{dvorak,ogloza}. However, it seems almost impossible to analyse the O--C diagram due to insufficient data. \citet{wolf} published $uvby-\beta$ photometric survey of southern eclipsing binaries including MQ~Cen and its color index. Up to now, to our knowledge, there has not been other study in the literature on the determination of the physical properties of the system.

\section{Observational Data}

\subsection{Photometry}\label{Photometry}

In this study, the new observations have been combined with collected photometric data from several sources (see Table \ref{table1}). Our observations were performed during three seasons using the CELESTRON CGE 1400 XLT 0.35\,m telescope at the South African Astronomical Observatory (SAAO), Sutherland. A Moravian Instrument G2-4000 model CCD camera equipped with \textit{vby} Str\"{o}mgren filters was attached to telescope. In one season, a Cassegrain 762/11430 with a Moravian Instruments CCD camera G2-402 and \textit{BVRI} Johnson filters were used. These observations were conducted mainly by JJ and JL. In total, 13\,546 individual measurements were taken from 2000 to 2017 (see Table \ref{table1} for details).

The data reduction and extraction of the magnitude for each photometric filter were performed by using the {\sc C-Muniwin}\footnote{http://c-munipack.sourceforge.net/} software. The software uses standard bias frames, dark subtraction and flat field division for the preparation of the CCD frames, and then performs synthetic aperture photometry to extract the magnitude.

Additional photometric data were obtained from previous surveys in order to be combined with the observations. In this study, photometric data from bright southern stars have been used from the All Sky Automated Survey (ASAS; \citealt{pojmanski}). In this survey a wide-field 200/2.8 instrument was used and provided photometric measurements in Johnson $V$ and $I$-bands with relatively high accuracy for MQ~Cen. New Supernovae data was found in ASAS using a Nikon AF-S NIKKOR 400mm f/2.8G~ED~VR~AF lens with a ProLine PL230 CCD camera from FLI, with back-illuminated CCD sensor \citep{shappee, kochanek}. The last source of photometric data used in this study was collected using the Optical Monitoring Camera on-board the ESA mission, \textit{INTEGRAL} \citep{OMC}. The instrument has an aperture of 50/154 mm and a CCD camera with a EEV 47-20 CCD chip used for photometry in the \textit{V}-band.

\begin{table*}
	\begin{center}
		\fontsize{10pt}{10pt}\selectfont
		\caption{Photometric data used in this study.}\label{table1}
		\begin{tabular}{lccc}
			\hline\hline
			Source & Filter & Time interval & Number of obs. \\
			\hline
			ASAS   & \textit{V}      & 51878.8-55048.5 & 523 \\
			       & \textit{I}      & 51869.9-53011.8 & 211 \\
			ASAS-SN & \textit{V}     & 57420.7-57926.6 & 718 \\
			OMC     & \textit{V}     & 52818.4-57781.2 & 375 \\
			SAAO    & \textit{v}     & 55694.4-56381.2 & 2295 \\
			& \textit{b}     & 55694.4-56381.2 & 2388 \\
			& \textit{y}     & 55694.4-56381.2 & 2366 \\
			& \textit{B}     & 55297.3-55307.7 & 1074 \\
			& \textit{V}     & 55294.4-55307.7 & 1252 \\
			& \textit{R}     & 55294.4-55307.7 & 1153 \\
			& \textit{I}     & 55294.4-55307.7 & 1191 \\
			\hline
		\end{tabular}
	\end{center}
\end{table*}

All the model parameters have been found by using a weighted robust regression method which eliminated relatively frequent outliers \citep{mik03}. The photometric observations and analysis have given a linear ephemeris of the MQ Cen binary system:

\begin{equation}\label{ephem}
\mathrm{Min I (HJD)}=2\,455\,696.4485(22)+3.686\,963\,1(9) \times E.
\end{equation}

The stability of the orbital period was tested and it was ascertained that $\dot{P}=2(3)\times10^{-9}$. Due to the small value obtained, when compared to the measured uncertainty (see Eq.~1), it could be pertinent to neglect it. The same argument can also be considered valid with the orbital eccentricity whereby because the secondary minimum light occurs at the orbital phase 0.50003(5), the orbital eccentricity can be considered zero.

\subsection{Spectroscopy}

The spectroscopic observations of MQ~Cen were made with the FEROS spectrograph on the 2.2\,m MPG/ESO telescope in La Silla, Chile. During five observing nights in March 2011, a total of 25 high-resolution $(R (\lambda / \Delta\lambda) \sim48\,000)$ spectra were collected. FEROS is fed by two fibers and each fiber is illuminated via 2.0~arcsec aperture, which means that the third light source detected in the photometry is not included in the composite spectra. The exposure times were set to 1200 s to obtain an average of S/N ratio of $\sim$120 at 6000 {\AA}. The {\sc IRAF} package was used for continuum normalization of the data reduction pipeline. For each telescope pointing, two consecutive exposures were taken to allow an estimation of the spectrum S/N ratio. This is accomplished by investigating the product of the division between the two consecutive spectra. Through this methodology, any spectral feature which originates from either the stellar atmospheres or from the interstellar medium, will cancel each other, leaving only the observational bias. In this way, the S/N ratio has been calculated for each spectrum at six different wavelengths to check the relative uncertainties in RV measurements.

Spectral lines of both components are clearly visible in the spectra, which allow the double-lined radial velocity curves of the system to be obtained. To disentangle spectral lines of both components, and to determine their radial velocities we used the code {\sc korel} \citep{hadrava} in {\sc vo-korel} implementation\footnote{see \url{https://stelweb.asu.cas.cz/vo-korel/}} \citep{skoda}. We have selected three spectral regions covering four strong spectral lines He 4471 {\AA} + Mg 4481 {\AA}, He 5875 {\AA}, and He 6678 {\AA}. The radial velocities and their uncertainties are given in Table \ref{table2}. Spectroscopic orbital solution obtained from {\sc korel} was combined with the fixed orbital period \textit{P} given in Eq. \ref{ephem} and by setting the eccentricity to zero (\textit{e} = 0) resulted in following values: $K_{1} = 158.9\pm0.8$ km s$^{-1}$, $K_{2} = 131.6\pm0.7$ km s$^{-1}$, $q = K_1/K_2 = 1.207\pm0.009$ and $V_\gamma = -1.2\pm4.8$ km s$^{-1}$.

It is known that the broad, overlapping spectral lines may cause incorrect orbital velocity determinations up to 2-3 per cent \citep[e.g.][]{popper}. This is the result of line core shifts when two broad lines overlap or blend, so that traditional RV measuring techniques like cross-correlation (e.g., fitting a Gaussian to line cores), gives an incorrect velocity. However, for modern techniques like spectral disentangling, the spectral lines of the components move along the wavelength axis to match the composite spectrum. In this case, it removes the effects from the overlapping of spectral lines in RV measurements, which makes it a very efficient tool for orbital parameter determination of double-lined spectroscopic binaries.

\begin{figure*}
	\begin{center}
		\begin{tabular}{cc}
			\resizebox{80mm}{!}{\includegraphics{fig2a.eps}} & \resizebox{80mm}{!}{\includegraphics{fig2b.eps}}\\
			\resizebox{80mm}{!}{\includegraphics{fig2c.eps}} &
			\resizebox{80mm}{!}{\includegraphics{fig2d.eps}}\\
			\resizebox{80mm}{!}{\includegraphics{fig2e.eps}} &
			\resizebox{80mm}{!}{\includegraphics{fig2f.eps}}\\
			\resizebox{80mm}{!}{\includegraphics{fig2g.eps}} &
			\resizebox{80mm}{!}{\includegraphics{fig2h.eps}}\\
			\resizebox{80mm}{!}{\includegraphics{fig2i.eps}} &
			\resizebox{80mm}{!}{\includegraphics{fig2j.eps}}\\

		\end{tabular}
		\caption{Disentangled spectral lines of MQ Cen components.}
		\label{fig2}
	\end{center}
\end{figure*}

\begin{table*}
	\begin{center}
		\fontsize{8pt}{10pt}\selectfont
		\caption{Journal of spectroscopic observations.}
		\label{table2}
		\begingroup
		\setlength{\tabcolsep}{4pt}
		\renewcommand{\arraystretch}{1.5}
		\begin{tabular}{lllcccccccccccc}
			\hline\hline
			ID &Observation &Phase & \multicolumn{4}{c}{HeI4471 {\AA} + MgII4481 {\AA}} & \multicolumn{4}{c}{HeI5875 {\AA}} & \multicolumn{4}{c}{HeI6678 {\AA}} \\
			&(HJD - & ($\phi$) & RV$_{1}$ & err & RV$_{2}$ & err & RV$_{1}$
			& err & RV$_{2}$ & err & RV$_{1}$ & err & RV$_{2}$ & err \\
			&2\,400\,000)&  & \multicolumn{2}{c}{km s$^{-1}$}
			& \multicolumn{2}{c}{km s$^{-1}$} & \multicolumn{2}{c}{km s$^{-1}$} &
			\multicolumn{2}{c}{km s$^{-1}$} & \multicolumn{2}{c}{km s$^{-1}$} &
			\multicolumn{2}{c}{km s$^{-1}$} \\
			\hline
			\,\,1 & 55647.6116&  0.753 & 158.0  & -0.7 & -132.4 & -0.8 & 156.3  & -2.4 & -133.7 & -2.2 & 156.6  & -2.2 & -138.8 & -7.3  \\
			\,\,2 & 55647.6261&  0.757 & 158.6  & 0.1  & -131.8 & -0.5 & 156.3  & -2.3 & -133.7 & -2.4 & 156.5  & -2.0 & -132.3 & -0.9  \\
			\,\,3 & 55648.4967&  0.993 & 14.5   & 11.0 & -2.3   & 0.6  & 5.7    & 2.3  & -1.8   & 1.0  & 3.2    & -0.3 & -1.9   & 0.9   \\
			\,\,4 & 55648.5112&  0.997 & -1.6   & -1.2 & 0.0 & -0.4 & 2.4    & 2.9  & 1.3    & 0.9  & 2.0    & 2.5  & -0.6   & -1.0 \\
			\,\,5 & 55648.5257&  0.001 & 6.9    & 11.3 & 4.8 & 1.2  & -4.6   & -0.2 & 3.7    & 0.1  & -4.4   & 0.0  & 3.1    & -0.5 \\
			\,\,6 & 55648.5402&  0.005 & -8.8   & -0.5 & 6.9 & 0.0  & -7.4   & 0.9  & 6.4    & -0.5 & -8.7   & -0.4 & 7.0    & 0.1   \\
			\,\,7 & 55648.5564&  0.010 & -7.1   & 5.5  & 10.1 & -0.4 & -13.7  & -1.1 & 10.2   & -0.3 & -13.1  & -0.4 & 10.8   & 0.3   \\
			\,\,8 & 55648.5709&  0.014 & -15.9  & 0.7  & 13.8 & 0.0  & -6.3   & 10.3 & 15.6   & 1.8  & -18.3  & -1.7 & 13.8   & 0.1   \\
			\,\,9 & 55648.5854&  0.017 & -16.1  & 4.4  & 15.9 & -1.1 & -19.0  & 10.5 & 16.6   & -0.4 & -21.2  & -0.7 & 17.8   & 0.8   \\
			10& 55648.5999&  0.021 & -16.7  & 7.7  & 21.3 & 1.1  & -24.0  & 0.4  & 21.2   & 1.0  & -26.2  & -1.8 & 21.2   & 1.0   \\
			11& 55648.6146&  0.025 & -22.3  & 6.1  & 22.2 & -1.2 & -26.7  & 1.6  & 25.8   & 2.3  & -28.4  & -0.1 & 23.7   & 0.3   \\
			12& 55648.6291&  0.029 & -35.7  & -3.6 & 26.1 & -0.6 & -31.4  & 0.8  & 26.3   & -0.3 & -33.6  & -1.4 & 28.7   & 2.1   \\
			13& 55649.5273&  0.273 & -156.5 & 0.2  & 129.9  & 0.0  & -156.6 & 0.2  & 130.9  & 1.1  & -157.1 & -0.4 & 129.6  & -0.3  \\
			14& 55649.5418&  0.277 & -157.5 & -1.4 & 129.9  & 0.7  & -156.2 & -0.2 & 129.0  & -0.3 & -156.2 & -0.2 & 130.1  & 0.8   \\
			15& 55649.6172&  0.297 & -150.3 & 0.6  & 126.0  & 0.9  & -151.2 & -0.3 & 126.1  & 1.0  & -151.2 & -0.3 & 126.2  & 1.1   \\
			16& 55649.6317&  0.301 & -149.9 & -0.2 & 125.9  & 1.9  & -150.1 & -0.4 & 126.2  & 2.2  & -156.3 & -6.6 & 126.2  & 2.2   \\
			17& 55650.4902&  0.534 & 42.0   & 5.2  & -30.0  & 0.5  & 37.4   & 0.5  & -31.2  & -0.7 & 36.9   & 0.0  & -31.2  & -0.7 \\
			18& 55650.5047&  0.538 & 54.0   & 13.4 & -32.8  & 0.8  & 40.6   & -0.1 & -33.6  & 0.0  & 41.2   & 0.6  & -34.2  & -0.6 \\
			19& 55650.5505&  0.550 & 53.4   & 0.9  & -45.1  & -1.7 & 52.7   & 0.2  & -46.0  & -2.5 & 53.1   & 0.6  & -43.7  & -0.3 \\
			20& 55650.5650&  0.554 & 57.9   & 1.7  & -46.9  & -0.3 & 55.2   & -1.0 & -47.1  & -0.6 & 56.2   & 0.1  & -48.0  & -1.5 \\
			21& 55650.7014&  0.591 & 89.8   & 0.9  & -73.2  & 0.4  & 89.1   & 0.2  & -73.2  & 0.5  & 88.9   & 0.0  & -73.7  & -0.1 \\
			22& 55650.7159&  0.595 & 90.4   & -1.7 & -77.3  & -1.0 & 91.7   & -0.4 & -76.5  & -0.2 & 91.6   & -0.6 & -78.2  & -1.9  \\
			23& 55651.4902&  0.805 & 148.4  & 0.1  & -122.1 & 0.7  & 148.1  & -0.2 & -123.0 & -0.2 & 148.6  & 0.4  & -122.0 & 0.9  \\
			24& 55651.5048&  0.809 & 146.1  & -0.7 & -121.8 & -0.2 & 147.0  & 0.1  & -122.9 & -1.3 & 146.6  & -0.2 & -121.5 & 0.1   \\
			25& 55651.5941&  0.834 & 135.9  & -0.1 & -112.8 & -0.2 & 135.8  & -0.1 & -112.6 & 0.0  & 136.1  & 0.2  & -117.8 & -5.2 \\
			\hline
		\end{tabular}
		\endgroup
	\end{center}
\end{table*}

The individual spectrum of the components was obtained by using the {\sc korel} code, with the orbital parameters derived in Section\,\ref{Photometry} and combined with the component light factors for the epoch at each observed spectrum derived from the light curve solution (see \S3). Fig. \ref{fig2} shows a selection of component spectra between $\lambda 3800-4300$\,{\AA}.

\section{Analysis of the Photometric Data}

Prior to analysis of the photometric data, it was checked to see if there were any light sources within 30~arcsec of MQ~Cen in the All-Sky Catalogue of Point Sources (2MASS) Collaboration catalogue \citep{cutri}. We found an object, 2MASS J11441637-6143033, at 12~arcsec south-east of MQ~Cen (Fig. \ref{fig3}). The magnitude differences between MQ~Cen and the third light source in $J$, $H$ and $K_s$-bands are 1.13, 0.58 and 0.50 mag, respectively, which correspond to 26\,\%, 37\,\% and 39\,\% light contribution to the total flux. MQ~Cen and its visual companion are observed by the \textit{Gaia} \citep{gaia} satellite. The magnitude difference in \textit{Gaia} \textit{G}-band is 2.448 mag which corresponds to 10\,\% light contribution of the visual companion to the total flux. Using the light contributions from \textit{G, J, H} and \textit{K}-bands, a third order polynomial function was fitted to obtain the light contributions for other bands used in our study (Fig. \ref{fig4}).

\begin{figure}
	\begin{center}
		\resizebox{50mm}{!}{\includegraphics{fig3.eps}}

		\caption{MQ~Cen and the third light source at 12'' South-East. The image dimension is 34'' $\times$ 31''.}\label{fig3}
	\end{center}
\end{figure}

\begin{figure*}
	\begin{center}
		\resizebox{80mm}{!}{\includegraphics{fig4.eps}}

		\caption{In percentage, light contribution of the visible companion versus wavelength. The observations are represented by filled circles, while, the open circles represent the calculated values obtained from the polynomial fit. For each data point the spectral band label is given.}\label{fig4}
	\end{center}
\end{figure*}

The multi-band photometric data described in \S2.1 were modeled using the 2003 version of the Wilson-Devinney light curve and radial velocity analysis code \citep[][]{wilson}. The code requires the temperature of one of the components as a priori to calculate the temperature of the other component. A more reliable and direct way to determine the temperature is through the modeling of the stellar spectrum with theoretical stellar atmosphere models.

We obtained a spectrum at the orbital phase $\phi\sim$\,0.0, where the less massive but hotter primary component is completely occulted and we only see the more massive but cooler secondary star.

In our study, a spectrum at the orbital phase $\phi\sim$\,0.0 has been obtained, where the less massive but hotter primary component is completely occulted, and we only see the more massive but cooler secondary star has been observed.

Therefore, this spectrum is suitable for determining the atmospheric parameters such as temperature, surface gravity, projected rotational velocity and micro-turbulance velocity. A grid of \citet{kurucz} model stellar atmospheres and synthetic spectra was created by using the {\sc atlas9} and {\sc synthe} codes, respectively. The best fitting stellar atmosphere models yielded $T_{\rm eff2} = 15\,000\pm500$~K, $\log~g$ = 3.4 (cgs units), $v_{\rm rot}\sin i$ = 100~km s$^{-1}$ for the secondary component. The micro-turbulence velocity was adopted to be $\zeta$ = 2.0~km s$^{-1}$. The uncertainties are the standard deviations of the parameters obtained from each line fitting. Some of the fitted stellar atmosphere models are shown in Fig. \ref{fig5}. The same temperature value has been obtained after using the Str\"{o}mgren colours of the system given by \citet{wolf}.

During the modeling of the light curves, the bolometric albedo and the gravity darkening exponents were set to 1.0 as suggested for early-type stars. The logarithmic Limb Darkening (LD) law was adopted and the LD coefficients were taken from \citet{vanhamme}. The detached configuration was first adopted to see if the components were inside or outside their Roche lobe limits. The light curve parameters conjunction time ($T_0$), orbital inclination ($i$), primary star effective temperature ($T_{\rm eff1}$), surface potentials ($\Omega_{\rm 1,2}$) and light contribution of the primary component ($L_1$) were allowed to vary while the orbital period ($P$), orbital eccentricity ($e$) and secondary star effective temperature ($T_{\rm eff2}=15000\,K$) were fixed. According to the best fit obtained with the light curve model, the orbital inclination indicates that, at total eclipse, the less massive primary component is within its Roche lobe limit while the more massive secondary star is almost filling its Roche lobe limit. The final light curve parameters have been presented in Table \ref{table3} and the model light curve together with the spectroscopic orbit are shown in Fig. \ref{fig6}.

\begin{figure*}
	\begin{center}
		\begin{tabular}{cc}
			\resizebox{120mm}{!}{\includegraphics{fig5.eps}}\\
		\end{tabular}
		\caption{Fitted synthetic spectra of selected spectral lines at the orbital phase $\phi=0.0$ for MQ~Cen.}\label{fig5}
	\end{center}
\end{figure*}

\begin{figure*}
	\begin{center}
		\begin{tabular}{c}
			\resizebox{100mm}{!}{\includegraphics{fig6a.eps}}\\
			\resizebox{100mm}{!}{\includegraphics{fig6b.eps}}\\
		\end{tabular}
		\caption{Best fitting models for the light curves (upper panel) and the spectroscopic orbit (lower panel).}\label{fig6}
	\end{center}
\end{figure*}

\begin{table*}
	\begin{center}
		\caption{Solution parameters for the light curve and radial velocity curve. Error in brackets quotes uncertainty in the last digit.}
		\label{table3}
		\begin{tabular}{lc}\hline\hline
			Parameter              &  Value \\
			\hline
			$P$ (days)             & \multicolumn{1}{c}{3.6869627(10)}  \\
			$T_0$ (HJD)            & 2455552.6599(3) \\
			$T_{\rm eff1}$(K)      &  \multicolumn{1}{c}{16\,600 (20)} \\
			$T_{\rm eff2}$(K)      &   15\,000   \\
			$q$                    &  \multicolumn{1}{c}{1.207} \\
			$V_\gamma$\,(km s$^{-1})$&  \multicolumn{1}{c}{--1.2} \\
			$L_{1}/L_{1+2}$ ($v$)  &   0.2254(1) \\
			$L_{1}/L_{1+2}$ ($b$)  &   0.2219(1) \\
			$L_{1}/L_{1+2}$ ($y$)  &   0.2155(1) \\
			$L_{1}/L_{1+2}$ ($B$)  &   0.2254(6) \\
			$L_{1}/L_{1+2}$ ($V$)  &   0.2184(5) \\
			$L_{1}/L_{1+2}$ ($R$)  &   0.2084(6) \\
			$L_{1}/L_{1+2}$ ($I$)  &   0.1920(5) \\
			$L_{3}/L_{1+2+3}$ ($v$)  &   0.04(1) \\
			$L_{3}/L_{1+2+3}$ ($b$)  &   0.05(1) \\
			$L_{3}/L_{1+2+3}$ ($y$)  &   0.06(1) \\
			$L_{3}/L_{1+2+3}$ ($B$)  &   0.04(1) \\
			$L_{3}/L_{1+2+3}$ ($V$)  &   0.06(1) \\
			$L_{3}/L_{1+2+3}$ ($R$)  &   0.09(1) \\
			$L_{3}/L_{1+2+3}$ ($I$)  &   0.14(1) \\
			$e$                    &  \multicolumn{1}{c}{0}
			\\
			$i$ $(^{o})$            &  87.0(2)   \\
			$\Omega_{\rm 1}$       	&  6.919(5)  \\
			$\Omega_{\rm 2}$      	&  4.481(7)  \\
			$\Omega_{\rm cr}$      	&  \multicolumn{1}{c}{4.080(1)} \\
			$ r_{1} $				&  0.1755(6) \\
			$ r_{2} $     		 	&  0.3453(3) \\
			\hline
		\end{tabular}
	\end{center}
\end{table*}

\section{Discussion}

\subsection{Astrophysical parameters and the distance to the system}

The astrophysical parameters of the MQ~Cen components are calculated and presented in Table \ref{table4}. The masses and the radii of the components are derived to within a precision of 1-2\,\% which allowed us to derive their spectral types. Following the table of fundamental stellar parameters given by \cite{straizys}, the mass of the secondary component implies a B4~V-IV star, however, its radius is $\sim$\,35 per cent larger than a normal main-sequence star, indicating an early departure from the main sequence. Nevertheless, the mass and radius of the less massive primary component indicate a typical B5 main-sequence star.

The color excess ($E(B-V)=0.34$ mag) obtained from Str\"{o}mgren colors in \S3 has yielded an estimate of the visual absorption between MQ~Cen and the Sun, as $A_V=0.34\times3.1=1.05$ mag. The absolute visual magnitude of the components was derived by using the bolometric magnitude and correction. The derived distance to MQ~Cen was found to be $d=$\,2.46\,$\pm$\,0.31\,kpc, using the system visual magnitude ($V=10.16$ mag), along with its absolute visual magnitude, visual absorption and the light contribution of the components.

The photometric distance found in this study appears to be slightly larger than the one reported in the \textit{Gaia} Data Release 2 (DR2) Catalogue \citep{gaia} (2.02\,$\pm$\,0.19 kpc), although they are in agreement regarding their uncertainties.

\begin{table*}
	\setlength{\tabcolsep}{3pt}
	\begin{center}
		\caption{Close binary stellar parameters of MQ~Cen. Uncertainty of each parameter is given in brackets.} \label{table4}
		\begin{tabular}{lccc}\hline\hline
			Parameter                 & Symbol  & Primary
			& Secondary     \\
			\hline
			Mass (M$_\odot$)          & \emph{M}& 4.26 (0.10)  & 5.14 (0.09) \\
			Radius (R$_\odot$)        & \emph{R}& 3.72 (0.05)  & 7.32 (0.03) \\
			Separation (R$_\odot$)    & \emph{a}& \multicolumn{2}{c}{21.2 (0.1)} \\
			Orbital inclination ($^{\circ}$) & \emph{i} & \multicolumn{2}{c}{87.0 (0.2)} \\
			Mass ratio                   & \emph{q} & \multicolumn{2}{c}{1.207 (0.009)} \\
			Eccentricity                 & \emph{e} & \multicolumn{2}{c}{0} \\
			Surface gravity             & $\log g$ & 3.926 (0.015)& 3.420 (0.014) \\
			Color index (mag)          & $B-V$ & \multicolumn{2}{c}{0.17 (0.06)} \\
			Intrinsic colour index (mag)& $(B-V)_{\rm0}$ &\multicolumn{2}{c}{--0.17}\\
			Color excess (mag)         &$E(B-V)$& \multicolumn{2}{c}{0.34}\\
			Visual absorption (mag)     & $A_{\rm v}$ &\multicolumn{2}{c}{1.05 (0.06)} \\
			Int. visual magnitude (mag)  & \emph{$V_{\rm0}$} &  \multicolumn{2}{c}{9.10 (0.09)} \\
			Temperature (K)       & $T_{\rm eff}$  & 16\,600 (520) & 15\,000 (500) \\
			Luminosity (L$_\odot$)      & $\log$ \emph{L}& 2.98 (0.08) & 3.39 (0.66) \\
			Bolometric magnitude (mag)  &$M_{\rm bol}$   & --2.70 (0.20) & --3.72 (0.17) \\
			Abs. visual magnitude (mag)  &$M_{\rm v}$  & --1.22 (0.21) & --2.48 (0.17) \\
			Bolometric correction (mag)   &\emph{BC}& --1.48 (0.07) & --1.24 (0.08) \\
			Velocity amplitudes (km\,s$^{-1}$)&$K_{\rm 1,2}$& 158.9 (0.8) & 131.6 (0.7) \\
			Systemic velocity (km\,s$^{-1}$)  &$V_{\gamma}$ & \multicolumn{2}{c}{--1.2 (4.8)} \\
			Computed sync. vel. (km\,s$^{-1}$)& $V_{\rm synch}$   & 59.7 (0.4) & 101.3 (0.7) \\
			Observed rot. vel. (km\,s$^{-1}$) & $V_{\rm rot}$ & 60 (2) & 100 (5) \\
			Distance (kpc) &\emph{d} & \multicolumn{2}{c}{2.46 (0.31)} \\
			\hline
		\end{tabular}
		\\Note: Solar units were used with following values: M$_\odot$ = 1.9891$\times$10$^{30}$ kg , R$_\odot$ = 695\,990 km, L$_\odot$ = 3.826$\times$10$^{26}$\,W.
	\end{center}
\end{table*}

\subsection{Evolutionary status of MQ~Cen}

Each component's evolutionary stage was investigated by locating its position on the HR diagram along with the theoretical evolutionary models (see Fig. \ref{fig7}). The PARSEC models have been adopted from \citet{bressan} for two different compositions (\textit{Z,Y}\,=\,0.008, 0.263 and 0.017, 0.279). The position of the components in the $\log T_{\rm eff} - \log L$ plane indicates that a more massive secondary component has already evolved from the main-sequence, while the primary star currently resides on the main-sequence. Taking into account the uncertainties of the derived parameters, both components lie within the age interval of 70 Myr.

\begin{figure*}
	\begin{center}
		\begin{tabular}{c}
			\hspace{1cm}
			\resizebox{100mm}{!}{\includegraphics{fig7.eps}}\\
		\end{tabular}
		\caption{Locations of the components of MQ~Cen in the log~$T_{eff}$ -- log~$L$ plane together with PARSEC evolutionary tracks and isochrones for \textit{Z}=0.017, \textit{Y}=0.279 (black) and \textit{Z}=0.008, \textit{Y}=0.263 (red).}\label{fig7}
	\end{center}
\end{figure*}

\subsection{Crux OB1 Membership}

The distance to MQ~Cen has been derived to be $d=$\,2.46 $\pm$\,0.31\,kpc in \S4.1, which is in agreement with the distance of the Crux OB1 association (2729 pc) determined by \citet{kaltcheva}. However, MQ~Cen with its age of $\tau_{MQ~Cen}\sim$\,70 Myr seems to be older than the age of the Crux OB1 association ($\tau_{Crux OB1}\sim$\,6.1\,$\pm$\,1.6 Myr \citep{kaltcheva}).

To determine the kinematical properties of MQ Cen, the velocity of the center of mass, the proper motion and the photometric parallax of the system have been used. The center-of-mass velocity ($V_{\gamma}=-1.2\pm4.8$ km s$^{-1}$) and the photometric parallax ($\pi=0.4065\pm0.051$ mas) of the system were evaluated in this study, whereas components of the proper motion ($\mu_{\alpha}\cos\delta$\,=\,--4.874\,$\pm$\,0.078, $\mu_{\delta}$\,=\,0.578\,$\pm$\,0.062 mas yr$^{-1}$) were taken from the {\em Gaia} DR2 Catalogue \citep{gaia}. The space velocity of the system, with respect to the Sun, was calculated using the algorithm described in \citet{johnson} where the space velocity components and their errors were found to be ($U$, $V$, $W$) = (--51.8\,3$\pm$\,6.80, -22.93\,$\pm$\,5.30, --8.10\,$\pm$\,1.26)\,km\,s$^{-1}$. The velocity components were corrected for the peculiar velocity of the Sun, which is known as (8.50\,$\pm$\,0.29, 13.38\,$\pm$\,0.43, 7.00\,$\pm$\,0.26)\,km\,s$^{-1}$ and is given by \citet{coskunoglu}. Therefore, the final Local Standard of Rest (LSR) space velocity components ($U$,$V$, $W$)$_{LSR}$ of MQ~Cen are (--43.33\,$\pm$\,6.81, --9.55\,$\pm$\,5.32, --1.61\,$\pm$\,1.29)\,km\,s$^{-1}$, respectively. The total space velocity of MQ~Cen is $S=44.40\,\pm\,8.74$ km s$^{-1}$. The total space velocity of the system is in agreement with the space velocities of young thin-disc stars \citep{legett}. In addition, the MQ Cen space velocity components obtained in this study, are close to the space velocity components (($U$, $V$, $W$) = (--43.7\,$\pm$\,1.6, -16.6\,$\pm$\,1.9, --6.2\,$\pm$\,0.8) km s$^{-1}$) calculated for the Crux OB1 by \citet{tetzlaff}. Interestingly, if the distance parameter of the system is taken as $\pi=0.4947\pm0.0499$ mas in {\em Gaia} DR2 catalogue \citep{gaia}, then the space velocity components of the MQ~Cen system would become ($U$, $V$, $W$)=(--42.68\,$\pm$\,4.76,--18.65\,$\pm$\,4.79, --6.66\,$\pm$\,0.90)\,km\,s$^{-1}$ which are more compatible with \citet{tetzlaff}. Kinematic analysis shows that MQ~Cen system is strong candidate for membership of the Crux OB1 association.

\section{Concluding Remarks}

Looking at what we have already explained, we conclude our study with the following remarks:

The astrophysical parameters of the massive early-type binary system, MQ~Cen have been determined to a precision of 1-2\,\% which allowed us to construct an evolutionary model for this system. According to the scenario, the more massive secondary component has completed the hydrogen burning phase (main-sequence life). As the secondary component evolves towards the giant branch, it will continue expanding, until reaching its Roche lobe limit in the future. This system is presently located just before the mass transfer stage. Later, it should reach the mass-ratio reversal stage, before becoming a classical Algol-type binary.

According to \citet{zahn}, the components of a binary system become tidally locked in spite of the synchronization of their axial rotation and orbit period. The synchronization time-scale is a function of physical properties of the components and the orbital period of the system. Using the physical properties of the components of MQ~Cen and following the methodology of \citet{zahn}, the synchronization time scale of MQ~Cen was found to be 2~Myr, which indicates that the system has completed synchronization about $\sim$70 Myr ago during the main-sequence lifetime. As expected, the measured rotational velocities of the primary and the secondary components are close to their calculated synchronization velocities (see Table \ref{table4}).

The sky position, the distance and the kinematical parameters of MQ~Cen are in good agreement with those of Crux OB1 association. However, the age of MQ~Cen seems to be larger than the age of Crux~OB1. Being aware of the existence of systems with similar ages would give clues about the existence of a different hierarchical stellar association in the vicinity of Crux~OB1. This would require more comprehensive and systematic observational studies over a relatively long period of time \citep[e.g.][]{pecaut}.

\textbf{Acknowledgements} The spectroscopic observations were performed under ESO grant number {\it 086.D-0236}. The work of ZM, JJ, MZ was supported by GA\,\v{C}R grant 16-01116S. This research has made use of ``Aladin sky atlas'' developed at CDS, Strasbourg Observatory, France. This work has made use of data from the European Space Agency (ESA) mission {\it Gaia} (\url{https://www.cosmos.esa.int/gaia}), processed by the {\it Gaia} Data Processing and Analysis Consortium (DPAC,  \url{https://www.cosmos.esa.int/web/gaia/dpac/consortium}). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the {\it Gaia} Multilateral Agreement. On the other hand, authors would like to express their warm thanks to Jeremy Tregloan-Reed (CITEVA, University of Antofagasta, Chile) and Ali Akbar Taheri (English Department at Bo\u{g}azi\c{c}i University, Turkey) for their help for correcting the English language and proof reading of the paper.

\begin {thebibliography}{}

\bibitem[Bak{\i}\c{s} et al.(2011)]{bakis11} Bak{\i}\c{s} H., Bak{\i}\c{s} V., Bilir S., Mikul\'{a}\v{s}ek Z., Zejda M., Yaz E., Demircan O., Bulut I. 2011, \pasj, 63, 1079
\bibitem[Bak{\i}\c{s} et al.(2014)]{bakis14} Bak{\i}\c{s} V., Hensberge H., Bilir S., Bak{\i}\c{s} H., Yilmaz F., Kiran E., Demircan O., Zejda M., Mikul\'{a}\v{s}ek Z. 2014, \aj, 147, 13
\bibitem[Bak{\i}\c{s} et al.(2015)]{bakis15} Bak{\i}\c{s} V., Hensberge H., Demircan O., Zejda M., Bilir S., Nitschelm C. 2015, ASP Conf. Ser., 496, 189
\bibitem[Bressan et al.(2012)]{bressan} Bressan A., Marigo P., Girardi L., Salasnich B., Dal Cero C., Rubele S., Nanni A. 2012, \mnras, 427, 127
\bibitem[Co{\c s}kuno{\v g}lu et al.(2011)]{coskunoglu} Co{\c s}kuno{\v g}lu B., Ak, S., Bilir, S., et al. 2011, \mnras, 412, 1237
\bibitem[Cutri et al.(2003)]{cutri} Cutri R. M., Skrutskie M. F., van Dyk S. et al. 2003, "The
IRSA 2MASS All-Sky Point Source Catalog, NASA/IPAC Infrared Science Archive
\bibitem[Dvorak(2004)]{dvorak} Dvorak S. W. 2004, IBVS, 5542, 1
\bibitem[Flower(1996)]{flower} Flower P. J. 1996, \apj, 469, 355
\bibitem[Gaia Collaboration (2018)]{gaia} Gaia Collaboration, A. G. A. Brown, A. Vallenari, T. Prusti et al. 2018,  \aap, 616, 22
\bibitem[Guthnick \& Prager(1934)]{guthnick} Guthnick P., Prager R. 1934, Astron. Nach., 251, 257G
\bibitem[Hadrava(1995)]{hadrava} Hadrava P. 1995, \aaps, 114, 393
\bibitem[Hog et al.(2000)]{hog} Hog E., Fabricius C., Makarov V. V., Urban S., Corbin T., Wycoff G., Bastian U., Schwekendiek P., Wicenec A. 2000, \aap, 355, 27
\bibitem[Humphreys(1978)]{humphreys} Humphreys R. M. 1978, \apjs, 38, 309
\bibitem[Johnson \& Soderblom(1987)]{johnson} Johnson D. R. H., Soderblom D. R. 1987, \aj, 93, 864
\bibitem[Kaltcheva \& Georgiev(1994)]{kaltcheva} Kaltcheva N. T., Georgiev L. N. 1994, \mnras, 269, 289
\bibitem[Kharchenko et al.(2005)]{kharchenko05} Kharchenko N. V., Piskunov A. E., R{\"o}ser S., Schilbach E., Scholz R. D. 2005, \aap, 438, 1163
\bibitem[Kochanek et al.(2017)]{kochanek} Kochanek C. S., Shappee B. J., Stanek K. Z., et al. 2017, \pasp, 129, 104502
\bibitem[Kouwenhoven et al.(2007)]{kouwenhoven07} Kouwenhoven M. B. N., Brown A. G. A., Portegies Zwart S. F., Kaper L. 2007, \aap, 474, 77
\bibitem[Legett(1992)]{legett} Leggett S. K. 1992, \apjs, 82, 351
\bibitem[Mikul\'a\v{s}ek(2015)]{mik15} Mikul\'a\v{s}ek, Z. 2015, \aap 584, A8
\bibitem[Mikul\'a\v{s}ek et al.(2008)]{mik08} Mikul\'a\v{s}ek Z., Krti\v{c}ka J., Henry G. W., et al. 2008, \aap, 485, 585
\bibitem[Mikul\'a\v{s}ek et al.(2003)]{mik03} Mikul{\'a}{\v s}ek Z., \v{Z}i\v{z}\v{n}ovsk\'{y} J., Zverko J., et al. 2003, Contr. Astron. Inst. Sk. Pleso, 33, 29
\bibitem[Kurucz(1993)]{kurucz} Kurucz R. L. 1993, CD-ROM 13, 18
\bibitem[Mas-Hesse et al.(2003)]{OMC} Mas-Hesse J. M., Gim{\'e}nez A., Culhane J. L., et al. 2003, \aap, 411, L261
\bibitem[Moon \& Dworetsky(1985)]{moon} Moon T. T., Dworetsky M. M. 1985, \mnras, 217, 305
\bibitem[Ogloza \& Zakrzewski(2004)]{ogloza} Ogloza W., Zakrzewski B. 2004, IBVS, 5507, 1
\bibitem[Pecaut \& Mamajek (2016)]{pecaut} Pecaut M. J., Mamajek E. E. 2016, \mnras, 461, 794
\bibitem[Pojmanski(2002)]{pojmanski} Pojmanski G. 2002, Acta Astron., 52, 397
\bibitem[Popper \& Hill (1999)]{popper} Popper D. M., Hill G. 1991, \aj, 101, 600
\bibitem[Shappee et al.(2014)]{shappee} Shappee B. J., Prieto J. L., Grupe D., et al. 2014, \apj, 788, 48
\bibitem[\v{S}koda et al.(2012)]{skoda} \v{S}koda P., Hadrava P., Fuchs J. 2012, \iaucirc, 282, 403
\bibitem[Straizys \& Kuriliene (1981)]{straizys} Straizys V., Kuriliene G. 1981, \apss, 80, 353
\bibitem[Tetzlaff et al.(2010)]{tetzlaff} Tetzlaff N., Neuh\"{a}user R., Hohle M. M., Maciejewski G. 2010, \mnras, 402, 2369
\bibitem[Tovmassian et al.(1996)]{tovmassian} Tovmassian H. M., Navarro S. G., Cardona O. 1996, \aj, 111, 306
\bibitem[van Hamme(1993)]{vanhamme} van Hamme W. 1993, \aj, 106, 2096
\bibitem[Wilson \& Devinney(1971)]{wilson} Wilson R. E., Devinney E. J. 1971, \apj, 166, 605
\bibitem[Wolf \& Kern(1983)]{wolf} Wolf G. W., Kern J. T. 1983, \apjs, 52, 429
\bibitem[Zahn(1977)]{zahn} Zahn J. P. 1977, \aap, 57, 383.

\end{thebibliography}

\end{document}

redpajama_set_name: RedPajamaArXiv


You are one of the many people who've discovered that Time Warner Cable is their cable television service provider in Ojai, CA. 94% of Ojai residents still watch their favorite television shows on a traditional screen; that's people. Perhaps you number among the remaining 6% who use their smartphones, computers and tablets to watch television programming each week. No matter how you like to watch TV, there are packages to fit your TV habits.
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(2) Whether desire is a cause of sorrow?
(3) Whether the craving for unity is a cause of sorrow?
(4) Whether an irresistible power is a cause of sorrow?
Whether sorrow is caused by the loss of good or by the presence of evil?
than by the presence of an evil. For Augustine says (De viii QQ. Dulcit.
like manner, every sorrow is caused by the loss of some good.
Q, A). Therefore sorrow is caused chiefly by the loss of good.
rather than for an evil that is present.
evil gives rise to fear, the present evil is the cause of sorrow."
chiefly, the present evil or the good which is lost.
lower place. But if we consider the cause of both these movements, viz.
the reason for its downward tendency.
says that pain results from the loss of temporal goods.
in a way, directed to the same thing under a contrary aspect.
which is suitable to it according to its own nature.
Whether desire is a cause of sorrow?
OBJ 1: It would seem that desire is not a cause of pain or sorrow.
one contrary is not a cause of movement towards the other contrary.
Therefore desire is not a cause of pain.
future. Therefore desire is not a cause of pain.
OBJ 3: Further, that which is pleasant in itself is not a cause of pain.
But desire is pleasant in itself, as the Philosopher says (Rhet. i, 11).
Therefore desire is not a cause of pain or sorrow.
is the cause of error. Therefore desire is a cause of sorrow.
the part of the end, the other, on the part of the principle of movement.
natural inclination resulting from gravity.
good which we desire to have.
causes the inclination of the appetite to fly from evil, as stated above.
reckoned as causing the appetitive movements that regard evil.
reckoned as present, and so gives rise to sorrow.
presence of an obstacle, desire causes sorrow.
Whether the craving for unity is a cause of sorrow?
"seems to have originated in pains and pleasures connected with food."
to unity, and division is the cause of multitude.
feeling of impatience of division or corruption?"
which its perfection consists: wherefore the Platonists held that "one"
for good is a cause of sorrow, so also is the love or craving for unity.
unity, but for that unity in which the perfection of nature consists.
connected with it, such as union of the sense to its object.
Whether an irresistible power is a cause of sorrow?
reckoned as a cause of sorrow.
the movements of appetite. But a greater power is something external.
Therefore it should not be reckoned as a cause of sorrow.
is caused by sense resisting a stronger body."
upward tendency is not violent but natural to it.
would be not sorrow but pleasure.
but actually, i.e. by causing the actual presence of the corruptive evil.
it cannot bring about that which causes sorrow.
greater power is reckoned to be the cause of sorrow.


Now that I am old and my hair is gray, don't leave me, God. I must tell the next generation about your power and greatness. God, your goodness reaches far above the skies. You have done wonderful things. God, there is no one like you.


text:
Crime + Justice Energy + Environment Extreme Weather Space + Science
NASCAR bans Confederate flags at all races, events
By Steve Almasy, CNN
Updated 11:29 PM EDT, Wed June 10, 2020
NASCAR driver to race with Black Lives Matter themed car
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On Monday, the only full-time African American driver in NASCAR's Cup Series called for the auto racing body to ban Confederate flags from its events. Two days later, his dream came true.
"The presence of the Confederate flag at NASCAR events runs contrary to our commitment to providing a welcoming and inclusive environment for all fans, our competitors and our industry," NASCAR said in a statement on its website hours ahead of its race Wednesday night in Martinsville, Virginia.
"Bringing people together around a love for racing and the community that it creates is what makes our fans and sport special. The display of the Confederate flag will be prohibited from all NASCAR events and properties."
This week, driver Bubba Wallace told CNN's Don Lemon he wanted NASCAR to go further than 2015, when it asked fans not to bring the Confederate flags to races.
HAMPTON, GEORGIA - JUNE 07: Bubba Wallace, driver of the #43 McDonald's Chevrolet, wears a "I Can't Breath - Black Lives Matter" T-shirt under his fire suit in solidarity with protesters around the world taking to the streets after the death of George Floyd on May 25 while in the custody of Minneapolis, Minnesota police, stands during the national anthem prior to the NASCAR Cup Series Folds of Honor QuikTrip 500 at Atlanta Motor Speedway on June 07, 2020 in Hampton, Georgia. (Photo by Chris Graythen/Getty Images)
Chris Graythen/Getty Images North America/Getty Images
Opinion: NASCAR does the right thing on Confederate flag ban
"No one should feel uncomfortable when they come to a NASCAR race. It starts with Confederate flags," Wallace said. "Get them out of here. They have no place for them."
Before Wednesday's race, Wallace told Fox Sports 1 that NASCAR made the right call.
"Bravo," he said while clapping. "Props to NASCAR and everybody involved. … There's a lot of emotions on the racetrack and off the racetrack that are riding with us. Tonight is something special. Today has been special. Hats off to NASCAR."
Wallace had told CNN that initially Confederate flags did not bother him, but after educating himself he sees how uncomfortable it makes people.
"There's going to be a lot of angry people that carry those flags proudly but it's time for change," he said.
At a race Sunday, Wallace wore a "I Can't Breathe" T-shirt in solidarity with protesters around the world who have been calling for justice in the death of George Floyd, an unarmed black man who died at the hands of Minneapolis police.
He wore the shirt again Wednesday.
A week after Floyd's May 25 death and amid massive protests for racial justice, NASCAR released a statement.
"For us to heal and move forward as a nation, we all need to listen more and be united in the stand against racism, hatred and senseless violence and loss of life. And we must all hold ourselves accountable to driving positive change." NASCAR said.
Charlotte Mayor Vi Lyles tweeted her appreciation.
"Thank you, NASCAR for doing the right thing. You are so central to our Carolina culture and I'm glad spectators and fans of all races, particularly Black fans like me, will feel more welcomed and respected at your events," Lyles tweeted.
The NASCAR Hall of Fame is in Charlotte, and nearly all of the sports' teams are based in the area.
Tennis legend Billie Jean King applauded the decision.
"It should have been done long ago," she tweeted. "Nonetheless, thank you, @NASCAR, for stepping out on the right side of history by banning Confederate flags at events and on properties."
#NASCAR, family...
— Be A King (@BerniceKing) June 10, 2020
Bernice King, daughter of Martin Luther King Jr., tweeted simply: "#NASCAR, family…"
Wallace raced a black car with the words "#blacklivesmatter" on it Wednesday night when he finished 11th.
In 2013, Wallace, 26, became the first African American driver since Wendell Scott (1963) to win an event sponsored by NASCAR when he won a trucks series race at Martinsville
Bubba Wallace, driver of the #43 McDonald's Chevrolet, wears an "I Can't Breath - Black Lives Matter" T-shirt under his fire suit in solidarity at Atlanta Motor Speedway on June 7, 2020.
NASCAR's Bubba Wallace will have Black Lives Matter paint scheme on car at Martinsville Speedway race
Martinsville is one of the tracks where Confederate flags are often seen in the parking lots and campgrounds, but Wednesday's race will have no fans.
NASCAR won't allow limited numbers of fans in the grandstands until Sunday at the Cup race in Homestead, Florida.
NASCAR was formed in 1948 and runs three national series – Cup, Xfinity and trucks.
CNN's Jill Martin, Dianne Gallagher and Amir Vera contributed to this report.

redpajama_set_name: RedPajamaCommonCrawl


Companies in the same industry as Garden Room, ranked by hourly rate.
How much does Garden Room pay?
Garden Room pays its employees an average of $14.00 an hour. Garden Room employees with the job title Accountant make the most with an average hourly rate of $22.10, while employees with the title Kitchen Assistant, Restaurant make the least with an average hourly rate of $10.51.


New York Times columnist Thomas Friedman often frustrates me with his breathless pronouncements, but in this long article, published back in April, he offers more than enough cogent points to make up for it.
Possibly interesting comments on gasoline prices.
On my professional blog, I wrote something that the folks here might find interesting. Note especially the couple of paragraphs of commentary at the very end.
Worldviews will often disagree, especially when there are interested parties on various sides with competing objectives. It's human nature. But the assumptions embedded in these worldviews deserve to be examined. […] Smart investors always look at both "upside potential" and "downside risk." When I read comments like Lundberg's, it seems to me that those who defend the status quo of the petroleum industry focus on potential and risk strictly for their own industry, without acknowledging the possible downside risks for the world at large.
It's blog-crossover madness, I tell you!
This week the Wall Street Journal ran an interesting interview with George David, the highly regarded chief executive of United Technologies Corporation. David is one of the all-stars of the corporate world: in the fifteen years that he's run UTC, the company's value has grown tenfold. Today its offerings include everything from Pratt & Whitney aircraft engines to Otis elevators.
One of the things that struck me in David's comments was his insistence on the importance of energy efficiency and conservation.
I think the solution to the energy problem is actually not alternative energy. To me, the solution immediately is conservation by greater efficiency. Too much in the mind of the public is this idea that conservation means deprivation. You've got to be cold at night, shut off the lights, stuff like that. That's simply not true. The bottom line is that energy is wasted in the world to a phenomenal extent. There's enormous energy savings potential in the conservation agenda where you do it by efficiency. In our own internal operations, we dropped the energy consumption at UTC by 19% over a decade at the same time the company doubled its size. All of America can drop its energy consumption by 20% in a decade easily. We're now working with the World Business Council for Sustainable Development to come up with a building that uses zero net energy.
This is music to my ears, especially considering its source. For myself, I think that the solution to our energy problems must include alternative sources of energy, but I also welcome mass adoption of David's view on the current level of waste in our human operations. The truth is, an abundance of cheap energy over the past century, while enabling huge strides in technology, global travel, and trade, has also instilled an ethic of waste in many of us. It has become incredibly easy and cheap — relative to the prior course of human history — to make more things, to ship them quickly, and then to whisk away the leavings. It has been incredibly easy to leave the lights on, and to build in pockets of waste in our systems, simply out of habit, or for want of better forethought. It has become normal to waste. Indeed, we have come to see it as our birthright, at least judging by the way that we cling to some of our old, wasteful habits. We stamp our feet and insist that we must be able to have our cake and eat it, too, because, because . . . well, we've just got to.
George David isn't buying it. He sounds like he wants a revolution in efficiency.
[Mr. David:] You can't walk through life with a trained eye and not see the opportunities for productivity. Every time you sit in traffic, that's a productivity loss. Every time you go to the doctor and fill out a bunch of forms and he refers you to somebody else and you fill out the same forms all over again, that's a loss of productivity. Whenever you wait for something, that's waste. I believe you can have 10 times more. I really do.
WSJ: Ten times more of what?
Mr. David: Everything. Everything. Just look at the differences in personal productivity between people, educated versus not educated. Or people in good, really productive labor environments, versus people who are kind of struggling because they're in disorganized or ineffective companies.
A large number of people have been deprived by opportunity, by education, by life's circumstance, and they end up having less than fully productive lives. It's not only bad for them as individuals, it's also very bad for the society because it's all lost work.
The whole interview is well worth reading. Now that I've read it, I'm thinking of all the areas of my own life — whether it's sitting in traffic or watching the paper recycling pile up in the garage — where a changed approach could radically lower the amount of waste, and lost productivity, that I see as normal.
Just a good, old-fashioned festival of links, is what it is.
What with it being Monday, and all, what say we just tidy up the links backlog, eh?
–A long and detailed post by Laree Draper about testing for heart health. This is a compelling subject for her because Dave Draper (her husband, and a great guy to read on anything to do with weightlifting) just had quadruple-bypass surgery.
–Thor of Satisfaction writes an excellent post on how Zappos' customer service drives the amazing success of their business. Sure, you could shop elsewhere for shoes, but knowing what you know from this post . . . why would you?
–The Zappos experience calls to mind a recent item by Joel Spolsky, the first item of which is labeled "Fix everything two ways". At his company, customer service reps do whatever it takes to fix a customer's immediate problem, but then also go the extra mile(s) to make sure that the same problem never recurs for anyone else. The iterative power of the thing is just stunning, or so says Spolsky.
–Austin Kleon posts an apt long quotation from Bruno Bettelheim, in which Bettelheim praises the utility of fairy tales for introducing children to some of the hard facts of life in a way they can digest.
This reminds me to spend more time with my kids and the d'Aulaires.
–I'm hoping that Kathy Sierra will return to blogging when she's ready to. I was thrilled to meet her at SXSW Interactive last month, and her devoted readers will be thrilled to have the continued benefits of her thinking. Meanwhile, the online hatred that led her to suspend blogging has drawn sustained attention, including this piece from the New York Times.
–Jon Lebkowsky points to efforts by Whole Foods Market and Green Mountain Energy to help customers reduce their carbon footprints.
Andrew Donoho on Austin's Resource Management Commission.
One of the many nifty people I met during SXSW Interactive was Andrew Donoho; we had a nice chat on the upstairs porch of Opal Divine's during the Worldchanging happy hour.
Andrew's particularly well suited to discuss this, since he is one of the citizen-commissioners on the Resource Management Commission. I share both his hope that Austin will do the right thing when it comes to neutralizing its carbon impacts, and the worry that, when push comes to shove, we the citizens, our public officials, or the folks at Austin Energy will shy away from footing the bill for it.
Following up from yesterday's longer post on Peak Oil, I note that this story from the New York Times gives lots of detail on the rise in secondary and tertiary production at older oil fields in the U.S. and beyond.
The short version: when oil prices stay high, and as technology improves, predictions rise for the amounts of oil that can be feasibly extracted from older fields.
N.b.: Daniel Yergin (author of The Prize) and his Cambridge Energy Research Associates firm, which are cited more than once in the article, are consistently bullish — very bullish — about the long-term ability of oil companies to produce more and more oil.
A little something on Peak Oil.
My friend Tom asked me to write here about the phenomenon of "Peak Oil," which reminded me how much I have to learn on the subject. For the moment, then, just a sketch.
Hubbert's peak can refer to the peaking of production of a particular area, which has now been observed for many fields and regions. "Peak Oil" as a proper noun, or Hubbert's peak applied more generally, refers to a singular event in history: the peak of the entire planet's oil production.
Domestic oil production within the United States peaked in the early 1970s, with many important ramifications for U.S. political economy, domestic and international. The jury is still out on dating of the global Peak Oil event, but it may be happening 'round about . . . now.
Why is it important? For a variety of reasons, but most importantly because cheap petroleum underlies so many aspects of modern industrialized life. The recent run of high oil prices reminds us of the many direct and indirect affects that oil price has on the economy. Yes, the price you pay for gasoline goes up, but so does the price you pay for airline tickets, UPS shipping, and a diverse range of other goods, from corn to kiwi fruit, that rely on cheap petroleum to be produced and delivered at low prices. Everyone agrees that high oil prices exert broad market effects; the big debate is over how dire these effects are, or will be, when Peak Oil is reached and the world petroleum industry truly goes into its long period if diminishing returns. For the moment, I'll simplify by saying that the scariest predictions are dire in the sense that, oh, The Black Death was "dire".
Where could I go to learn more? The Wikipedia entry already referenced has a lot of information, plus many links to other sources. Read it all with a grain of salt and remember that there are fundamental disagreements about when the Peak comes and what the Peak means when it comes. (If you detect a note of apocalyptic language here, you're onto something.) Another good place to start, if you want a ton of information on the subject delivered daily, is The Oil Drum. The folks who write it take the existence and the broad threat of Peak Oil for granted. They have organized a useful primer on the subject, which they call "The Book". This takes you through many, many aspects of petroleum production and pricing, and the impacts of these on — well, on just about everything. They guys use copious graphs, by the way.
There are also a number of useful books on the subject, many of which are listed at the bottom of the Wikipedia entry. I would start with Twilight in the Desert by Matthew Simmons. The book is about the decline of production that Simmons perceives in the oil fields of Saudi Arabia. Simmons is a favorite of the Peakers (as Peak Oil buffs are often called) because he has for many years run a Houston-based investment bank dedicated to making deals in the oil industry; ergo, he's an insider, and can't be brushed aside lightly by those (inside the oil business or out) who categorically deny the threat posed by Peak Oil. Also worth your while are Hubbert's Peak and Beyond Oil by the eminent professor of petroleum geology Kenneth Deffeyes. Deffeyes thinks we're in pretty big trouble. Another notable voice on this subject is James Howard Kunstler, who has long been a critic of American suburban sprawl, and who wrote the influential book The Long Emergency about what he sees as the coming oil crunch. You will very quickly come to grasp his approach and tone if you read his site.
So, that's hardly a comprehensive introduction, but at least it can serve as a placeholder for further discussions later.


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HomeDid Moses Have a Speech Impediment?
Did Moses Have a Speech Impediment?
PhilologosSeptember 9, 2011
An interesting query comes from Gerald M. Siegel, professor emeritus in the Department of Speech, Language, and Hearing Sciences at the University of Minnesota. He writes:
In the Torah [Exodus 4:10], Moses initially resists being God's messenger because of his speech, saying: "Please, O Lord, I have never been a man of words…. I am heavy of mouth and heavy of tongue." From this the rabbis concluded that Moses was a stutterer, which a story in the midrash attributes to his having burned his tongue on hot coals as an infant. Yet why decide that he stuttered rather than that he suffered from some other speech impediment? On what basis was this explanation given?
Actually, there has been a wide gamut of rabbinical interpretations of the Hebrew words k'vad peh, "heavy of mouth," and k'vad lashon, "heavy of tongue," by which Moses describes himself. If that of stutterer has become the most accepted, this is probably because it is found in the 11th-century commentary of Rabbi Shlomo Yitchaki or Rashi, the most popular of all Jewish biblical exegetes. As is sometimes his manner, Rashi translates the Hebrew into medieval French, in this case using the noun balbus, stuttering or stammering (from which comes the modern French verb balbutier, to stutter), to which later glossarists added the Old German Stammeler, a stutterer.
Yet this was only one opinion. Abraham Ibn Ezra, writing several decades after Rashi, thought otherwise. In his commentary on the Bible, also widely used to this day, he writes:
And whoever says that he [Moses] had forgotten the Egyptian tongue is mistaken…. He was not referring to that, but rather… to being unable to produce all the sounds made with the tongue and the lips, only some of which he could articulate with difficulty.
Ibn Ezra, in other words, did think that Moses had a speech impediment other than stuttering, although precisely what it was, he didn't say. (The theory, dismissed by Ibn Ezra, that Moses' problem was having forgotten to speak Egyptian during his long sojourn in Midian, to which he fled after killing an Egyptian taskmaster as a young man, can be found in a bibli cal commentary by Rashi's grandson, the 12th-century Rabbi Shmuel ben-Meir, or Rashbam.)
The first commentator to speculate what this impediment might have been was Bahye ben Asher — better known as Rabbeinu Bahye — who lived in the last half of the 13th and first half of the 14th century. Taking "heavy of mouth" and "heavy of tongue" not as mere poetic parallelisms but as linguistically precise terms, he took the former to refer to an inability to sound palatal consonants like "z," "s," "sh," and "ts," and the latter to a similar difficulty with apico-dentals like "d," "t" and "l." Needless to say, anyone with so many speech difficulties would be all but incomprehensible, which Moses quite obviously wasn't, but perhaps Bahye meant only that he suffered from one in each category.
The well-known midrash cited by Professor Siegel does not point to stuttering as Moses' problem, either. According to this legend, Moses — an exceptionally beautiful and precocious baby raised by Pharaoh's daughter at her father's court — kept reaching for the king's crown, causing Pharaoh's counselors to urge killing him, since they feared this signified that he would cleverly usurp Pharaoh's place when he grew up.
The decision was then taken to test Moses' intelligence by presenting him with a golden bowl and an even more brightly glowing coal to see which he chose — and when, his hand guided by an angel, he grabbed the coal, thereby flunking this primitive IQ test, his life was spared. Sticking his burned finger in his mouth, however, he scorched his tongue too, as a result of which his speech was permanently impaired.
A damaged tongue, one would think, would be more likely to cause lisping than stuttering. And there were yet other rabbinic commentators who denied that Moses had any speech impairment at all and who took "heavy of tongue" and "heavy of mouth" to indicate verbal slowness and deliberateness, so that what Moses was saying to God was that he could not talk glibly or smoothly enough to be a successful leader. Indeed, the first-century C.E. Aramaic translation of the Bible known as Targum Onkelos, which preserves some of the oldest rabbinic interpretations to have come down to us, characterizes Moses' speech as profound, rendering k'vad peh as yakir mamlal, "weighty of speech," and k'vad lashon as amik lishan, "deep of tongue," turning Moses' negative self-description into a positive one.
Still, the popular perception of Moses as a stutterer persists, as is made manifest by the newly formed Jewish Stuttering Association, an American self-help organization that calls itself in Hebrew Mercaz Kvad Peh, "The K'vad Peh Center." Moses' stuttering is even said to have cost the Jews dearly. When offered by God the choice of any country in the world, a modern midrash goes, he meant to request vast, rich Canada but was given tiny, resourceless Canaan when all he could manage to utter was "C-C-Cana-C-C-Cana…." It's equally likely, though, that he asked for the Land of Ithrael and got exactly what he wanted.
Questions for Philologos can be sent to philologos@forward.com
Philologos


These four films (The Battle of Megiddo, Tombrobbers, Murder in the Temple, The Twins) tell the true stories of real people who lived in ancient Egypt thousands of years ago. This is the story of ancient Egypt from the ground up: the real lives of humble quarrymen, devious aristocrats, dutiful daughters and conquering Pharaohs. Their narratives, and their own words, have come down to us in a handful of rare documents, letters, and other intimate records which open a window into this ancient world. This is an ancient Egypt that has not been seen before: intimate, visceral, and above all human, peopled by characters whose passions and pre-occupations we recognize today.


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The Unsubtle Sphinx
by A C Spahn
A. C. Spahn wanted to be an interstellar starship captain when she grew up. Since nobody was hiring, she became a writer instead. She enjoys training in martial arts, organizing messy rooms, and researching a hobby-of-the-month. When not commanding imaginary starships, she lives in Pennsylvania with her husband, son, and feline overlord. She is the author of the Endurance series of comedic sci-fi novellas and short stories appearing in Outposts of Beyond, Disturbed Digest, and other publications.
"I've figured out what you are," said Detective Derek Faraday.
Cara Watt, paranormal investigator, paused just outside the crime scene tape line. "I beg your pardon?"
"I know what kind of paranormal creature you are." Derek's triumphant grin brought a boyish gleam to his handsome features.
Cara planted her hands on her hips. "All right, what am I?"
"You're a siren. You help me on cases, but only because you're luring me to trust you before you strike and kill me."
"No," Cara said, chuckling, "I'm not a siren, Derek."
"I notice you didn't say you aren't planning to kill me."
Cara ducked under the crime scene tape. "If you thought I was going to kill you, you wouldn't keep calling for my help."
"Fair enough." Derek gestured to the building in the center of the taped-off area. "Help me with this one, then? I'm still getting used to the, er, colorful citizens in this town."
Together they rounded the building, a squat little sandwich shop with a purple awning and a ring of outdoor picnic tables. The entrance to the shop was a single glass door, leading to a cramped counter and two narrow indoor tables.
Blocking the door sat the reason for the crime scene tape. Cara pulled up short when they came within view. "Oh no. Not again."
It was a massive lion, haunches positioned before the doorway, tail tapping the asphalt. Its shoulders brushed the purple awning. It turned to face them as they approached, revealing a humanoid head atop the feline body. The features were feminine, with a haughty intellect behind the eyes.
"Sphinx?" Derek asked quietly. Cara nodded. "Am I right in guessing it's blocking the way into Santos' Subs because it has a riddle for us to answer?"
"Most likely. This is Axura. She shows up every couple weeks and gets in everybody's way."
"I can hear you," the sphinx said, her voice deep enough to jostle the nearby trees.
Slowly the detective and investigator approached. Axura swished her tail, raised her chin, and said, "What walks on four legs in the morning--"
"A human," said Cara and Derek together.
Axura huffed. "Fine. If you've heard that one before, I'll give you another. Answer me correctly, and I'll stop blocking this door:
Bender of light,
Enabler of sight,
Solid as a wall,
Except when I fall.
What am I?"
"Now wait a minute," said Derek, reaching for his badge. "On behalf of the owner of this establishment, I'm going to need you to move, riddle or no riddle. You can't justa--"
Axura growled. The sound rolled across the pavement and shuddered the windows in their frames. Derek went completely still.
"Answer," said Axura, "or I will eat you."
"Never argue with a sphinx," Cara whispered. "It won't end well. I have an answer to the riddle. Do you?"
Derek waved for Cara to speak, his eyes still fixed on the enormous creature who hadn't quite ceased growling.
Cara stepped forward. "It's glass," she said. "It refracts light, is see-through, forms a solid barrier, but shatters when it falls over."
Axura's shoulders stiffened. "How did you know?"
"It might have helped if you weren't sitting right in front of a glass door," said Derek. Another growl silenced him.
Axura huffed again as she stood. She arched her back in a luxurious stretch against the shop awning as she slunk out into the open. "Go on in, then," she said. "I shall find another place to lurk." She paced away, tail swishing irritably and flicking leaves from trees.
"I'm guessing we'll see her again," Derek said.
Cara nodded. "Unfortunately, yes. Hopefully she doesn't realize riddles work best when the answer isn't hiding in plain sight."
Derek eyed the purple awning, which still clutched a few strands of fur. "Since we're here... can I buy you a sandwich?"
"No longer worried I'm plotting your demise?"
"If you are, I doubt you're planning to murder me with ham and cheese on sourdough. You'd go for something more subtle."
Cara laughed and hooked her arm through his. "You don't know me half as well as you think you do. It'd be ham and cheese on rye."
The Cara Watt stories were inspired by the two-minute mysteries by Donald J. Sobol, featuring Dr. Haledijan the sleuth solving various cases alongside the reader. My husband and I enjoyed reading Dr. Haledjian's adventures aloud together, and the pairing of the interactive mystery style with a paranormal setting seemed like a perfect fit.
- A C Spahn
We hope you're enjoying The Unsubtle Sphinx by A C Spahn.


I'm really fired up to share this with you. Our fearless leader was recently a guest on Radio BrendoMan Episode 364 – Check it out to hear more of our founder's story and the road that lead to starting myopic studios.
Huge shout out to Brendo for inviting Pete on the show! Get out there and show Brendo and his team some love.


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Touring and concerts
Bangin' on the beach in the East River: Electric Zoo Festival.
Where once electronic dance music (EDM) filled a fashionable niche, it has now achieved critical mass. Nowhere is this better exemplified than this year's Electric Zoo on Randall Island New York which returned on Labor Day weekend with an ever more robust line up of the world's leading names in EDM. The highest grossing EDM artist in the US for 2012 Tiësto is joined by Axwell from Swedish House Mafia; and Steve Aoki to name just three. "Along with the producers, we organize events of this scale worldwide and draw on a wealth of experience in this genre," said sound specialist George Stavro of Sonic Lab Audio and Integral Sound, "And we contract in what we know to be the best equipment to make the weekend fizz."
Stavro projects as a typically plain speaking Australian sound man, but beneath his leathery left field humor there lurks a specialist of remarkable technical proficiency. "There are three of us at Integral Sound to oversee this event; Steve Dash, a legend in EDM from the very early days, Mike Bindra our event production guru, and myself with a specialty in sound system design and configuration. For Electric Zoo I've specified loudspeaker systems from d&b audiotechnik for all four venues on the island: Main Stage, Riverside Stage, Sunday School and Hill Top.
With EDM shows, if it's done well it gives people a sense of joy and elation; that's what we specialize in. But when you're listening to EDM for a sustained period as you are during the three days of Electric Zoo then ear fatigue can become a problem. To counter this we have developed a specific PA tuning regime that relieves the condition without any compromise to the listening experience. That might sound a little glib, but think of the d&b systems as the canvas for a painter; our special tuning is the layers of wash an artist will apply to present a specific luminosity in the finished work. The thing is, when you apply specific tuning to a PA it can badly influence performance elsewhere in the audio system: but not with the d&b systems. Although I specialize in EDM I've worked with all kinds of live music and I find with d&b systems their inherent response is so smooth, even and consistent, that it doesn't matter what art form you apply, it will always perform beautifully. The d&b J-Series is the prime component for three of the four venues and is typical; a loudspeaker system that is absolutely flat straight out of the box, allowing me to make the EQ lifts and cuts that suit EDM and delivers that bangin' experience without overburdening the senses of our audience."
"We subcontract Eighth Day Sound for all the equipment, all to our specification," said Stavro. "They supply all the J-Series, as well as elements of Q and C-Series, and the large quantities of subs we need, including the notorious d&b B2-SUB, which we use in CSA mode to great effect." Stavro creates defined sub-arcs across the front of all the stages neatly avoiding the bludgeoning tunnel of power that can easily sap the energy from the audience core. The main J-Series systems are flown high to enable maximum downward tilt, "It might be an island but we don't want to upset the neighbors across the river," said Stavro. "With the pattern control these systems achieve we also avoid coloring the adjacent stages. Some people think what we do is pretty unorthodox but as I said, it's what we're known for, and it works."
Products employed
J8 loudspeaker
J12 loudspeaker
J subwoofer
B2 subwoofer
Heritage product
Q1 loudspeaker
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A vision of Britain through time
A vision of Britain from 1801 to now.
Including maps, statistical trends and historical descriptions.
Help using this website
Statistical atlas
Burton upon Trent PLU/RegD
Poor Law Union/Reg. District
Relationships and changes
Available Themes
Densities and rates of growth. Age structure: concentrations of young people, and of the old.
How people made their living: identifying farming communities, pit villages, mill towns and so on.
Numbers of babies born. Deaths, especially infant deaths. Causes of death by age and gender.
Numbers of houses. Overcrowding: persons per room. Amenities: central heating, baths and WCs.
Click on the hyperlinks for direct access to key graphs and tables.
Total Population 1801 to 1911: Population grew from 19,679 in 1801 to 92,160 in 1911.
Age Structure, in 5-year bands, from 1851 to 1911: In 1851, 5.6 per cent of the population were aged 65 and over, but by 1911 only 5.15 per cent were.
Infant Mortality Rate 1871 to 1911: The highest rate recorded was 131.82 infant deaths per thousand live births in 1871, and the lowest was 107.96 in 1901.
Occupational Structure in 1881:
Here we are presenting statistics for a historical unit, which may have changed its boundaries significantly during the period covered.
Preferred Name:
Registration District
Poor Law Union
Date abolished:
Unit ID:
Authorities:
F. Youngs, Local Administrative Units: Northern England (London: Royal Historical Society, 1991), p. 742.
Burton upon Trent PLU/RegD, Staffordshire
We know of no alternate names.
Unit associations
We know of no associations with other units.
Unit history
This unit was part of the following units:
STAFFORDSHIRE Poor Law/Registration County 1850 F. Youngs, Local Administrative Units: Northern England (London: Royal Historical Society, 1991), p. 742.
We know of no boundary changes affecting this unit.
Lower level units
This unit contained the following units:
BURTON UPON TRENT Registration sub-District 1911 Census of England and Wales, Table 5, 'Registration Counties, Districts and Sub-districts with their constituent civil parishes. - Urban or Rural District in which each parish is situated; Area; families or separate occupiers, and population, 1901 and 1911; and population enumerated in Institutions, large establishments, and on vessels, &c., 1911'.
GRESLEY Registration sub-District 1911 Census of England and Wales, Table 5, 'Registration Counties, Districts and Sub-districts with their constituent civil parishes. - Urban or Rural District in which each parish is situated; Area; families or separate occupiers, and population, 1901 and 1911; and population enumerated in Institutions, large establishments, and on vessels, &c., 1911'.
REPTON Registration sub-District 1911 Census of England and Wales, Table 5, 'Registration Counties, Districts and Sub-districts with their constituent civil parishes. - Urban or Rural District in which each parish is situated; Area; families or separate occupiers, and population, 1901 and 1911; and population enumerated in Institutions, large establishments, and on vessels, &c., 1911'.
TUTBURY Registration sub-District 1911 Census of England and Wales, Table 5, 'Registration Counties, Districts and Sub-districts with their constituent civil parishes. - Urban or Rural District in which each parish is situated; Area; families or separate occupiers, and population, 1901 and 1911; and population enumerated in Institutions, large establishments, and on vessels, &c., 1911'.
ANSLOW CP/Tn Parish-level Unit 1866 F. Youngs, Local Administrative Units: Northern England (London: Royal Historical Society, 1991), p. 402.
ASH CP/Hmlt Parish-level Unit 1837 1930 F. Youngs, Local Administrative Units: Northern England (London: Royal Historical Society, 1991), p. 66.
BARTON BLOUNT AP/CP Parish-level Unit 1837 1930 F. Youngs, Local Administrative Units: Northern England (London: Royal Historical Society, 1991), p. 67.
BARTON UNDER NEEDWOOD Ch/CP Parish-level Unit 1866 F. Youngs, Local Administrative Units: Northern England (London: Royal Historical Society, 1991), p. 402.
BEARWARDCOTE Tn/CP Parish-level Unit 1837 1930 F. Youngs, Local Administrative Units: Northern England (London: Royal Historical Society, 1991), p. 67.
BRANSTON Tn/CP Parish-level Unit 1866 F. Youngs, Local Administrative Units: Northern England (London: Royal Historical Society, 1991), p. 404.
BRETBY Ch/CP Parish-level Unit 1866 F. Youngs, Local Administrative Units: Northern England (London: Royal Historical Society, 1991), p. 69.
BURNASTON Tn/CP Parish-level Unit 1866 F. Youngs, Local Administrative Units: Northern England (London: Royal Historical Society, 1991), p. 69.
BURTON EXTRA Tn/CP Parish-level Unit 1866 1904 F. Youngs, Local Administrative Units: Northern England (London: Royal Historical Society, 1991), p. 406.
BURTON UPON TRENT CP/AP Parish-level Unit F. Youngs, Local Administrative Units: Northern England (London: Royal Historical Society, 1991), p. 406.
CALDWELL Hmlt/CP Parish-level Unit 1866 F. Youngs, Local Administrative Units: Northern England (London: Royal Historical Society, 1991), p. 69.
CASTLE GRESLEY Hmlt/CP Parish-level Unit 1866 F. Youngs, Local Administrative Units: Northern England (London: Royal Historical Society, 1991), p. 76.
CATTON CP/Tn Parish-level Unit 1837 1930 F. Youngs, Local Administrative Units: Northern England (London: Royal Historical Society, 1991), p. 70.
CHURCH BROUGHTON CP/AP Parish-level Unit F. Youngs, Local Administrative Units: Northern England (London: Royal Historical Society, 1991), p. 69.
CHURCH GRESLEY AP/CP Parish-level Unit F. Youngs, Local Administrative Units: Northern England (London: Royal Historical Society, 1991), p. 76.
COTON IN THE ELMS Tn/CP Parish-level Unit 1866 F. Youngs, Local Administrative Units: Northern England (London: Royal Historical Society, 1991), p. 71.
DALBURY LEES AP/CP Parish-level Unit F. Youngs, Local Administrative Units: Northern England (London: Royal Historical Society, 1991), p. 72.
DRAKELOW Tn/CP Parish-level Unit 1866 F. Youngs, Local Administrative Units: Northern England (London: Royal Historical Society, 1991), p. 74.
DUNSTALL Tn/CP Parish-level Unit 1866 F. Youngs, Local Administrative Units: Northern England (London: Royal Historical Society, 1991), p. 410.
EGGINTON AP/CP Parish-level Unit F. Youngs, Local Administrative Units: Northern England (London: Royal Historical Society, 1991), p. 74.
ETWALL CP/AP Parish-level Unit F. Youngs, Local Administrative Units: Northern England (London: Royal Historical Society, 1991), p. 75.
FINDERN CP/Ch Parish-level Unit 1866 F. Youngs, Local Administrative Units: Northern England (London: Royal Historical Society, 1991), p. 75.
FOREMARK CP/AP Parish-level Unit F. Youngs, Local Administrative Units: Northern England (London: Royal Historical Society, 1991), p. 75.
FOSTON AND SCROPTON CP/Tn Parish-level Unit 1866 F. Youngs, Local Administrative Units: Northern England (London: Royal Historical Society, 1991), p. 75.
HANBURY AP/CP Parish-level Unit F. Youngs, Local Administrative Units: Northern England (London: Royal Historical Society, 1991), p. 412.
HARGATE MANOR CP/ExP Parish-level Unit 1862 1885 F. Youngs, Local Administrative Units: Northern England (London: Royal Historical Society, 1991), p. 76.
HATTON Tn/CP Parish-level Unit 1866 F. Youngs, Local Administrative Units: Northern England (London: Royal Historical Society, 1991), p. 77.
HIGHLANDS PARK ExP Parish-level Unit 1891 Census of England and Wales, Table 2, 'Area and Population in Registration Districts and Sub-Districts and in Civil Parishes'.
HILTON CP/Tn Parish-level Unit 1866 F. Youngs, Local Administrative Units: Northern England (London: Royal Historical Society, 1991), p. 77.
HOON Tn/CP Parish-level Unit 1866 F. Youngs, Local Administrative Units: Northern England (London: Royal Historical Society, 1991), p. 77.
HORNINGLOW Tn/CP Parish-level Unit 1866 1904 F. Youngs, Local Administrative Units: Northern England (London: Royal Historical Society, 1991), p. 414.
INGLEBY Tn/CP Parish-level Unit 1866 F. Youngs, Local Administrative Units: Northern England (London: Royal Historical Society, 1991), p. 78.
LINTON Tn/CP Parish-level Unit 1866 F. Youngs, Local Administrative Units: Northern England (London: Royal Historical Society, 1991), p. 78.
LULLINGTON CP/AP Parish-level Unit F. Youngs, Local Administrative Units: Northern England (London: Royal Historical Society, 1991), p. 79.
MARSTON ON DOVE AP/CP Parish-level Unit F. Youngs, Local Administrative Units: Northern England (London: Royal Historical Society, 1991), p. 79.
MICKLEOVER AP/CP Parish-level Unit 1968 F. Youngs, Local Administrative Units: Northern England (London: Royal Historical Society, 1991), p. 80.
NEWTON SOLNEY CP/AP Parish-level Unit F. Youngs, Local Administrative Units: Northern England (London: Royal Historical Society, 1991), p. 81.
OSLETON AND THURVASTON Tn/CP Parish-level Unit 1837 1930 F. Youngs, Local Administrative Units: Northern England (London: Royal Historical Society, 1991), p. 82.
OUTWOODS CP Parish-level Unit 1894 F. Youngs, Local Administrative Units: Northern England (London: Royal Historical Society, 1991), p. 419.
RADBOURNE CP/AP Parish-level Unit F. Youngs, Local Administrative Units: Northern England (London: Royal Historical Society, 1991), p. 83.
REPTON AP/CP Parish-level Unit F. Youngs, Local Administrative Units: Northern England (London: Royal Historical Society, 1991), p. 83.
ROLLESTON CP/AP Parish-level Unit F. Youngs, Local Administrative Units: Northern England (London: Royal Historical Society, 1991), p. 420.
ROSLISTON Ch/CP Parish-level Unit F. Youngs, Local Administrative Units: Northern England (London: Royal Historical Society, 1991), p. 83.
SCROPTON AP/CP Parish-level Unit 1866 F. Youngs, Local Administrative Units: Northern England (London: Royal Historical Society, 1991), p. 421.
STANTON AND NEWHALL Tn/CP Parish-level Unit 1866 F. Youngs, Local Administrative Units: Northern England (London: Royal Historical Society, 1991), p. 85.
STAPENHILL CP/AP Parish-level Unit 1904 F. Youngs, Local Administrative Units: Northern England (London: Royal Historical Society, 1991), p. 85.
STRETTON CP/Tn Parish-level Unit F. Youngs, Local Administrative Units: Northern England (London: Royal Historical Society, 1991), p. 424.
SUTTON ON THE HILL CP/AP Parish-level Unit F. Youngs, Local Administrative Units: Northern England (London: Royal Historical Society, 1991), p. 86.
SWADLINCOTE Tn/CP Parish-level Unit F. Youngs, Local Administrative Units: Northern England (London: Royal Historical Society, 1991), p. 86.
TATENHILL CP/AP Parish-level Unit F. Youngs, Local Administrative Units: Northern England (London: Royal Historical Society, 1991), p. 425.
TRUSLEY CP/AP Parish-level Unit F. Youngs, Local Administrative Units: Northern England (London: Royal Historical Society, 1991), p. 86.
TUTBURY CP/AP Parish-level Unit F. Youngs, Local Administrative Units: Northern England (London: Royal Historical Society, 1991), p. 426.
TWYFORD AND STENSON Ch/CP Parish-level Unit 1866 F. Youngs, Local Administrative Units: Northern England (London: Royal Historical Society, 1991), p. 86.
WALTON UPON TRENT CP/AP Parish-level Unit F. Youngs, Local Administrative Units: Northern England (London: Royal Historical Society, 1991), p. 87.
WILLINGTON AP/CP Parish-level Unit F. Youngs, Local Administrative Units: Northern England (London: Royal Historical Society, 1991), p. 87.
WINSHILL Tn/CP Parish-level Unit 1866 1904 F. Youngs, Local Administrative Units: Northern England (London: Royal Historical Society, 1991), p. 88.
WYCHNOR Ch/CP Parish-level Unit F. Youngs, Local Administrative Units: Northern England (London: Royal Historical Society, 1991), p. 430.
How to reference this page:
GB Historical GIS / University of Portsmouth, Burton upon Trent PLU/RegD through time | Census tables with data for the Poor Law Union/Reg. District, A Vision of Britain through Time.
URL: http://www.visionofbritain.org.uk/unit/10005656
Date accessed: 17th January 2021
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Swiss superautomatic manufacturer Eversys is carving a niche for itself by creating machines with the soul of a barista in the body of an automatic coffee maker.
While coffee lovers in mature markets such as Europe and the US are beginning to expect high quality coffee in almost every imaginable setting (work, home, in transit), the need for new solutions for creating that coffee is growing ever stronger.
That is where technology comes in – with companies such as Eversys creating compact, reliable superautomatic machines that can provide barista-quality coffee at the touch of a button.
Swiss manufacturer Eversys has been built upon the vision of transforming the espresso machine market by challenging the traditional versus superautomatic equipment divide, says the company's Chief Commercial Officer Kamal Bengougam.
"Eversys was founded in 2009, a company with old heads yet young hearts and minds," Bengougam tells Global Coffee Report.
Given that the company has experienced consistent year-on-year growth every year it has been in operation, perhaps that ambition is not too far-fetched.
At its outset, Eversys launched its e'4 range of equipment.
Built around the e'Barista system, Eversys' machines produce coffee in a way that mirrors the traditional barista method, with electronic grinder adjustment, precision-driven brewing, extraction optimisation and thermodynamic integrity to produce consistently high quality coffee.
Since the company launched, it has enhanced its offering with the addition of such features as a one-step offering focusing on steamed milk products, connectivity with field-based equipment, mobile solutions such as integrated payment systems, self-service functionality and real-time data mining.
In 2014, Eversys also released the Shotmaster, a compact superautomatic machine that is capable of delivering four espressos at a time while using just 28 centimetres of bench space.
Like all Eversys machines, the Shotmaster uses a reverse extraction principle that gives it the ability to produce traditional standard espresso by extracting the product against gravitational forces.
The machine also incorporates Eversys's telemetry system, e'Connect, which won a Smart Label Award at the 2013 Host exhibition in Milan and provides all the information needed by professionals to manage their machine in real time via the internet.
The e'Connect system gives stakeholders the ability to remotely access information about all of the key parameters of the machines. This includes monthly, daily and even hourly productivity reports, feedback on technical performance and drink profiles. All of this information can be accessed through either push or pull functions, in line with the preference of the user.
Eversys' machines are also built using modular technologies, with all the main functionalities separated to provide ease of access and minimise downtime. Each machine consists of five modules – the grinder, the patented brewing module, the hydraulics, the steam and water boilers and the milk module.
The grinder module is made of two ceramic grinder discs, driven by a powerful yet quiet motor, whose heat is channelled away from the coffee beans via a set of fans. Electronic control maintains consistency of product throughout the day, ensuring optimal extraction at all times.
The brewing module uses a system of reverse gravity extraction vertical infusion to optimise powder efficiency as the espresso is produced.
The coffee boiler is kept separate from the water and steam boiler to provide greater temperature control and increase the productivity of the machine.
The machines also include Eversys' unique e'clean technology. Eversys machines can store one month's worth of cleaning tablets, dispensed daily through a laser guided automatic distribution unit. This ensures that health and safety standards are maintained, as well as safeguarding the machine's optimum performance.
Bengougam says that Eversys' target market is the discerning customer seeking to enhance their value offering, providing differentiation through genuinely creative solutions.
"The people who understand the difference between price and value," he says.
Being a company driven by quality, Bengougam says Eversys will appeal to those for whom the details really matter, organisations who derive both pride and profits from providing a great customer experience.
It is these qualities that Bengougam says he expects will stand his company in good stead as the industry grows ever more competitive.
Bengougam says that this ties in with the growth of consumer knowledge at a retail level, which has been propelled forward by the specialty coffee movement and its promotion by mainstream players such as Starbucks.
This has also led to an increasing sophistication in automatic machines built for the domestic market, leading to a blurring of the lines between the machines that are pitched at the domestic consumer and those, such as Eversys', which are designed primarily for the corporate market.
"In my opinion, the battle zone is being developed at the lower end of the market where home appliances companies are vying for entry into the lucrative lower end of the professional equipment market," Bengougam says.
But it is in the retail and corporate markets that Eversys has focused its efforts, anticipating and responding to a desire from an increasingly discerning consumer for creative new concepts from the convenience segment of the market, challenging the traditional coffee chains with both competitive pricing and quality offerings.
In the corporate market, Bengougam sees environmental considerations such as the carbon footprint of machines being a driving factor.
But ultimately, it is the result in the cup that will continue to drive Eversys forward.
"In-cup quality and consistency will always be paramount to our value offering as will enhanced connectivity [such as] distance diagnostics, real time data [and] remote access," Bengougam says.