text:
\section{Introduction} \label{sec:intro}
Metals are produced through nucleosynthesis, but the location and time of metal formation by stellar populations throughout cosmic history is still uncertain.
The hot halos of clusters are X-ray emitting extended components in which $>$80 \% of the baryons reside for high-mass clusters ($M_{500} > 10^{14} M_\odot$; \citealp{Andreon2010, Dai2010, KraBor2012}).
These clusters are considered to be closed systems that have retained nearly all their baryons, making their halos the ideal place for studying their stellar and elemental history.

The measured metallicities ($Z$) in the halos of high- and low-mass ($10^{13} M_\odot < M_{500} < 10^{15} M_\odot$) clusters are the same, even though the ratio of stellar mass to gas mass in high-mass clusters (stellar fraction, $M_*/M_{gas}$) is an order of magnitude lower than that of low-mass clusters \citep{Bregman2010, Lui2020}.
\cite{Loew2013} used the standard single-slope Salpeter initial mass function (IMF), applied specifically above the core-collapse mass cutoff, to derive an expected intracluster medium (ICM) metallicity from the current stellar populations of $Z_{Fe,ICM} = 0.106(10f_*/f_{ICM})$ where $f_*/f_{ICM} = M_*/M_{ICM} = M_*/M_{gas}$, using \cite{AndGrev1989} abundances.
For a cluster with $M_*/M_{gas}=0.02$ the expected ICM enrichment from the stellar populations is 0.021 $Z_\odot$.
Considerations such as the efficiency of  Type Ia and core-collapse supernova and a single high-redshift population of stars went into the prediction of observed ICM metallicity, but the measured metallicity is approximately four times greater than what is predicted \citep{Portarini2004, Loew2006, Siv2009, Bulbul2012, Loew2013}.
This is the missing metal conundrum.

We consider several possible explanations for the metal conundrum, but find a fault to each.
The first theory is that stars may exist in the ICM that produced a sufficient amount of metals to supply high-mass clusters with the measured ICM metallicity \citep{Renzini&Andreon2014}.
\cite{Siv2009} calculated the average metal contribution from intracluster stars with a standard IMF to be 25\% of the total ICM metallicity within $R_{500}$.
In order for intracluster stars to supply the missing metals, we would expect to find at least four times the intracluster stellar population (based on the metal contribution by \cite{Siv2009}).
Intracluster light in high-mass clusters represents approximately 20\% of the total cluster light \citep[e.g.,][]{Zibetti2005, Krick2007, Giallongo2014, Furnlell2021}.
A population four times larger, a sufficient size to account for the missing metals, would produce at least 80\% of the total cluster light.

The second theory considers a correlation between the IMF of the star-forming clouds at $z \sim 2$ and the final cluster mass \citep{Renzini&Andreon2014}.
High-mass clusters require an additional source of metals that are not produced by their visible stellar populations.
These metals could be formed by star-forming clouds at high redshift before the formation of galaxy clusters.
However, high-mass clusters require a greater source of metals from star-forming clouds than low-mass systems \citep[][and references therein]{Renzini&Andreon2014}.
The IMF of the star-forming clouds at high redshift would need to compensate for the missing metals by forming more high-mass stars for high final mass systems, and fewer high-mass stars for low final mass systems.
In order for this to be plausible, the star-forming clouds would have to ``know" the final mass of the future cluster, which is unlikely.

A favorable explanation for the metal conundrum is an early enrichment population (EEP); a population of stars that supplied high-mass clusters with most of their measured ICM metals \citep{Elbaz1995, Loew2001}.
This theory has been proposed through the study of halo metallicity evolution as a function of redshift \citep{Mantz2017, Flores2021} and cluster stellar fraction ($M_*/M_{gas}$; \citealp{Bregman2010}).
The EEP would have existed at high redshift, composed of primarily early Population II stars, which dominated during the reionization period $\sim6 < z < 10$, and favored a bottom-light IMF \citep{Fan2006, Loew2013, Planck2016reionization}.
The EEP would have occurred in nascent galaxies and not be prominent as $L^*$ galaxies, or be visible today \citep{WerMer2020}.
This solution avoids problems such as excess intracluster light and halo mass-IMF correlation in high-redshift star-forming clouds.

A few constraints are imposed on the EEP based on current observations.
The metallicity of high $M_*/M_{gas}$ systems cannot exceed observations, enforcing a maximum EEP metallicity ($Z_{EEP}$).
Limits of the mass of the EEP population ($M_{EEP}$) are imposed as the addition of the EEP and its remnants cannot exceed the cosmic baryon mass.

The need for this population is shown by plotting the $Z_{tot}$ against $M_*/M_{gas}$ \citep[e.g.,][]{Bregman2010}.
We use this methodology to place further constraints on the EEP, such as the supernova (SN) rate and total population mass.
The high-mass galaxy cluster RX J1416.4+2315 (hereafter RXJ1416) at $z \sim 0.137$ has $M_*/M_{gas} = 0.054 \pm 0.018$ \citep{Khosr2006, Bregman2010, Harrison2012}.
RXJ1416 is also classified as a fossil system (FS), which is an extreme subset of galaxy clusters \citep{Khosr2006}.
FS are suspected to be highly evolved galaxy groups and clusters dominated by a brightest central galaxy (BCG).
The official definition of these systems is generally accepted to be several distinguishing characteristics: (i) a magnitude gap of at least two between the brightest and second brightest members, (ii) both members are within half the virial radius, and (iii) the presence of a diffuse X-ray halo with $L_X \geq 10^{41} h_{70}^{-2}$ erg s$^{-1}$ \citep{Jones2003, Aguerri2011, Aguerri2021}.
Although the definition has been largely agreed upon, many defining factors of FS are unknown or debated, including the formation pathway, the average ICM metallicity, and the radial metallicity trend \citep{Donghia2005, VonBenda2008, Dariush2010}.

Current studies of FS suggest an overabundance of the ICM metallicity \citep[i.e.,][]{Khosr2006}.
This trend lends to the EEP theory, and an early formation of FS as present-day low surface brightness galaxies in FS may have formed alongside the EEP and then evolved to express the defining characteristics of FS.
We study the ICM metallicity of RXJ1416 and include it in the relation of $M_*/M_{gas}$ versus $Z_{tot}$ from \cite{Bregman2010}, from which we can derive the metal contribution from the EEP ($Z_{EEP}$) to the total metallicity ($Z_{tot}$) of the cluster.
We present derived observational quantities of the SNe rate and the total mass of the population from $Z_{EEP}$.

In Section \ref{sec:data} we discuss our handling of the X-ray data from which values presented in Section \ref{sec:spectral_analysis} are extracted.
These values are used to derive observational quantities of the EEP in Section \ref{sec:EEP_quantities}, and we summarize our findings in Section \ref{sec:summary}.

Throughout our study, we adopt a $\Lambda$CDM cosmology with $H_0 = 70$ km s$^{-1}$ Mpc$^{-3}$, a baryon density parameter of $\Omega_b = 0.0455$, dark matter density parameter of $\Omega_{DM} = 0.243$, and the total baryon density parameter is $\Omega_m = 0.288$ \citep{Planck2018cosmo}.

\section{Data Reduction and Analysis}\label{sec:data}

RXJ1416 is a fossil galaxy cluster - a highly relaxed and undisturbed galaxy cluster with an absolute magnitude gap of at least 2 between the brightest and second brightest galaxy \citep{Ponman1994, JoPoFo2000, Jones2003}.
This cluster has been studied and characterized by previous authors \citep{Khosr2006, Khosh2007} using X-ray data and by \cite{Cyp2006} using optical data.
The first two references provide radial kT measurements for comparison, $M_{200} = 3 (\pm 1) \times 10^{14} M_\odot$ and $R_{500} = 880 kpc$.
We used archival observations of RXJ1416 from XMM-Newton and Chandra to obtain radial kT and $Z_{tot}$ measurements from the system.
Final good-time intervals for data used are presented in Table \ref{tab:gti}.
In addition to XMM-Newton and Chandra data, we included a ROSAT All-Sky Survey (RASS) spectrum to better constrain the diffuse, soft X-ray background.

One further consideration that must be discussed is the value of $M_*$ for RXJ1416.
This value is not reported for the entire cluster, so it must be determined with the data provided.
A reasonable method for determining $M_*$ would be using a provided mass-to-light ratio (M/L) for galaxy clusters.
However, RXJ1416 is an FS, as determined by \cite{Khosr2006}, so typical M/L ratios of galaxy clusters cannot be used as the M/L ratio for FS is known to be higher than that of typical galaxy clusters, but how high is under dispute \cite[e.g.,][]{Vik1999, Sun2004, Khosh2007, Aguerri2021}.
Thus, the $M_*$ of RXJ1416 must be determined for the M/L ratio of the cluster itself.
\cite{Harrison2012} studied the BCG of RXJ1416 and determined $M_{*,BCG} = 1.08 \times 10^{12} M_\odot$ and $L_{BCG} = 3.53 (\pm 0.10) \times 10^{11} L_\odot$.
The M/L ration is then $3.06 (\pm 0.09) M_\odot/L_\odot$ for the BCG.
We use the M/L ration determined and the total \textit{r}-band luminosity within $R_{200}$ for the cluster from \cite{Khosr2006}, $L_{R,R_{200}} = 10^{11.85} L_\odot$, to calculate $M_{*,200} = 2.17(\pm 0.06) \times 10^{12} M_\odot$.
This results in a stellar fraction $M_*/M_{gas} = 0.054 \pm 0.018$.

\begin{table}[]
    \centering
    \caption{Good-time Intervals after cleaning data for XMM-Newton and Chandra detectors.}
    \begin{tabular}{c  c  c  c  c  c}
        XMM Newton & & & & Chandra & \\
        \hline
         OBSID & MOS1 & MOS2 & PN & OBSID & ACIS-I \\
         \hline
         0722140401 & 27 ks & 27 ks & 17.5 ks & 16125 & 31.73 ks \\
    \end{tabular}
    \label{tab:gti}
\end{table}

\begin{figure*}
    \centering
    \includegraphics[width=1\linewidth]{regions.png}
    \caption{Left: XMM-Newton Mos1 27 ks exposure image of RX J416.4+2315. Not shown, 10$\arcmin$-14$\arcmin$ background region. Right: Chandra ACIS-I chip 30 ks exposure image of RX J1416.4+1315. The same regions are shown on each chip - five annuli from which spectra were extracted and jointly fit. The outermost annuli is of radius $R_{500} = 5.33\arcmin$ \citep{Khosh2007}.}
    \label{fig:rxj_3region}
\end{figure*}

\subsection{XMM Newton Data Reduction}\label{XMM_Analysis}
RXJ1416 was observed by XMM Newton on four separate occasions.
Three of the four observations were dominated by soft proton flares, so we limited our study to observation 0722140401 (34 ks exposure before cleaning).
We followed the techniques outlined by \cite{Snowden2008}, the XMM-ESAS Cookbook\footnote{https://heasarc.gsfc.nasa.gov/docs/xmm/esas/cookbook/}, and the Extended Source Analysis Software (xmm-esas, SAS version 18.0.0)\footnote{https://www.cosmos.esa.int/web/xmm-newton/sas} for data extraction and reduction.
We examined the resulting light curves to ensure all flare intervals were excluded from the cleaned observations.
After cleaning, there were 27 ks, 27 ks, and 17.5 ks of good time available for the MOS1, MOS2, and PN instruments, respectively.
We used the filtered data sets for source and background data extraction, and the creation of response matrices and ancillary response files applied to the spectra.

We accounted for two known background and instrumental effects in data reduction and spectral fitting.
The finite point
spread function (PSF) of the XMM-Newton EPIC chips covers multiple annuli in which we extracted spectra of RXJ1416.
This allows for cross talk between the regions; an X-ray photon originating in one extraction annulus on the sky may be detected in another extraction annulus on the chip.
To account for this, we used the SAS command \textit{arfgen} to generate PSF maps between the multiple annuli and account for excess flux generated by X-ray photons detected in annuli from which they do not originate.
The PSF maps were included in the spectral fitting.

A second consideration involves only the PN instrument.
To improve counting statistics and energy range, we extracted two spectra from the same region.
A low-energy spectrum ($0.3 < E < 2.0$ keV) excluded a low-energy noise tail, and a high-energy spectrum ($1.0 < E < 8.0$ keV) maximized the number of events included at high energies.
During spectral extraction of the PN spectra, we set CCD PATTERN$<= 0$ for the low-energy spectra, and CCD PATTERN$<= 4$ for the high-energy spectra.

XMM Newton EPIC cameras have a field of view of 30$\arcmin$.
RXJ1416 has $R_{500} = 5.33\arcmin$ and is centered on CCD1 for the MOS instruments, quadrant 1 for the PN.
We defined an on-chip background region annulus of 10$\arcmin$-14$\arcmin$ outside of detectable cluster emission to better constrain the background emission. A prominent background source was noted and excluded during spectral extraction.
This source is located in defined extraction regions at coordinates (-463,-897) on MOS1 with a radius 2.5$\arcmin$, circled in white in Figure \ref{fig:rxj_3region}.

\subsection{Chandra Data Reduction}\label{Chandra Analysis}
RXJ1416 has been observed six times by Chandra.
Two of the six observations are centered on RXJ1416 and were 81.14 ks (observation ID 16125) and 14.57 ks (observation ID 2024) before filtering.
We used observation 16125 only as the observation was made in VFAINT mode, which has a 5x5 pixel event island instead of a 3x3 event island, allowing for better discrimination between X-rays and cosmic rays.
Additionally, the good time available from 16125, 31.73 ks, is more than double the unfiltered observation time of 2024.
We followed the data reduction procedure outlined by the Extended Source Analysis Guide\footnote{https://cxc.cfa.harvard.edu/ciao/guides/esa.html}.
All data reduction was performed in CIAO (version 4.12)\footnote{https://cxc.cfa.harvard.edu/ciao/releasenotes/ciao\_4.12\_release.html}, and used the most recent calibration files, CALDB (version 4.9.3)\footnote{http://cxc.harvard.edu/caldb/}.
We reprocessed the raw data to Level 2 event files, from which we extracted spectra and light curves to ensure all flare intervals are properly filtered.
We used the CIAO command \textit{wavedetect} to identify and remove point sources from the image.
The total exposure time available after reprocessing the data was 31.73 ks.
To properly account for the background, we generated blanksky\footnote{http://cxc.cfa.harvard.edu/ciao/threads/ acisbackground/} background files using an event file excluding point sources and flares.
Background spectra were extracted in the same detector region as the spectra from the blanksky background.

\begin{figure}[h]
    \centering
    \includegraphics[width=0.9\linewidth]{XMM_15-3.pdf}
    \caption{Spectral fit of the $0.15<R/R_{500}<0.30 $ region from XMM Newton. There are four spectra from the region of interest, one each from MOS1 and MOS2, and two from PN, shown in black, red, green (soft energy), and blue (hard energy), respectively.}
    \label{fig:xmm_spec}
\end{figure}

\section{Spectral Analysis}\label{sec:spectral_analysis}
Observational metallicity and plasma temperature trends have been determined and established for numerous galaxy clusters \citep[e.g.,][]{Vik2006, Burns2010, Reiprich2013, WerMer2020}.
Comparison of these trends determined for RXJ1416 against the known trends is necessary to corroborate the determined extraction method and determined values.

For XMM Newton and Chandra, we split up data extraction regions of RXJ1416 for concentric annuli simulated by a beta model to give similar signal-to-noise ratios.
The defined extraction regions, shown in Figure \ref{fig:rxj_3region}, are $R/R_{500}<0.15$, $0.15<R/R_{500}<0.30$, $0.30<R/R_{500}<0.55$, $0.55<R/R_{500}<0.75$, and $0.75<R/R_{500}<1.0$, where $R_{500} =$880 kpc \citep{Khosh2007}.
We fit the Chandra and XMM Newton spectra independently in the energy range $0.6 - 7.0$ keV using XSPEC (version 12.11.1)\footnote{https://heasarc.gsfc.nasa.gov/xanadu/xspec/}.
Five gaussian lines with fixed energy values are included to account for XMM Newton instrumental lines and solar wind charge exchange.
Normalization and width are initially fit and then frozen.
A total of three APEC models are used to account for various background X-ray sources, including the Local Hot Bubble, Milky Way halo emission, and the superposition of unresolved background emission.
An additional APEC model is used to constrain the plasma temperature and metallicity of the cluster halo.
Galactic absorption was accounted for using the XSPEC tbabs model set to a fixed column absorption value of $2 \times 10^{20}$ cm$^{-2}$ \citep{Khosh2007}.
We also include constants accounting for calibration differences between instruments and solid angle normalization to allow simultaneous parameter fits using multiple spectral extraction regions.
A power law is used for the emission from extragalactic active galactic nuclei with index 1.46 and a broken power law for any residual soft proton background emission.
We adopt the solar ratios of \cite{AndGrev1989} for all spectral fits.

\begin{figure}[h]
    \centering
    \includegraphics[width=0.9\linewidth]{Chandra_15-3.png}
    \caption{Spectral fit of the $0.15<R/R_{500}<0.30 $ region from Chandra.
    \label{fig:chandra_spec}}
\end{figure}

Fitting a region from XMM Newton includes more spectra than Chandra spectra due to special considerations of the PSF and PN counting statistics.
Each extraction region includes four spectra: MOS1, MOS2, soft-PN, and hard-PN.
Neighboring regions, the on-chip background (10-14'), and a ROSAT spectrum to better constrain the soft thermal emission component are fit simultaneously with the primary region.
The inner ($<0.15$ $R_{500}$) and outermost ($0.75<R/R_{500}<1.0$) extraction regions have a single neighboring region, meaning that 13 spectra are simultaneously fit for each region.
All other regions have two neighboring extraction regions, so 17 spectra are fit simultaneously.
Figure \ref{fig:xmm_spec} shows an XMM Newton spectral fit of the $0.15 < R/R_{500} < 0.3$ region.
Not shown in this fit are the spectra from the neighboring regions, on-chip background spectra, the on-chip background region, and ROSAT spectra.

We do not have to implement as many considerations when fitting Chandra spectra.
The PSF of the Chandra ACIS-I chip is approximately 1$\arcsec$ \footnote{https://cxc.harvard.edu/proposer/POG/html/chap6.html}, a much smaller area than the width of our defined extraction regions.
A single spectrum is extracted for each defined extraction region and fit simultaneously with a ROSAT spectrum.
Figure \ref{fig:chandra_spec} shows a Chandra spectral fit excluding the ROSAT and background spectra.

\subsection{Metallicity}\label{sec:metallicity}

Metallicity in a relaxed cluster is centrally peaked due to emission from the BCG, then sharply declines, and then remains constant beyond $\sim 0.3$ $R_{500}$ \citep{DeGrande2004, Merniew2018, Lov2019}.
We obtain $Z_{tot}$ measurements in predefined radial bins out to $R_{500}$ for XMM Newton and $0.55$ $R_{500}$ for Chandra.
Spectral fits are not obtained at larger radii for Chandra as high backgrounds dominate the spectra and the signal-to-noise ratios decrease to $< 0.5$ for $Z$ and kT.

We obtain $Z_{tot}$ measurements from extraction regions $0.3<R/R_{500}<0.55$,  $0.55<R/R_{500}<0.75$, and $0.75<R/R_{500}<1$.
For XMM Newton, we find $Z_{tot}=0.32 \pm 0.073$ $Z_\odot$, $Z_{tot}=0.40\pm0.13$ $Z_\odot$, and $Z_{tot} = 0.14 \pm 0.13$ for the three regions, respectively.
Metallicity measurements are determined only in the region $0.3< R/R_{500} < 0.55$ for Chandra, $Z_{tot} = 0.32 \pm 0.15$ $Z_\odot$.
We calculate a mean of the values weighted by the errors to combine all measurements from Chandra and XMM Newton resulting in a metallicity in annulus $0.3<R/R_{500}<1$ of $0.303 \pm 0.053$ $Z_\odot$.
We note that \cite{Khosh2007} measured an average $Z_{tot} = 0.23 \pm 0.07$ $Z_\odot$ within 0.45$R_{500}$ RXJ1416 obtained by spectral fitting of Chandra data.
This value is within $\sim$1$\sigma$ of the metallicity determined in radial region $0.3-0.55$ $R_{500}$, $0.31 \pm 0.073$.
Because the calibration changes were most likely not included in the errors, we find these measurements in agreement with each other.
All fit results are presented in Table \ref{tab:all_measurements}.

\begin{table*}[]
    \hspace{-1.5cm}
    \centering
    \caption{Metallicity and Plasma Temperature Values from spectral fits in defined regions from both XMM and Chandra.     \textbf{Note.} All errors on spectral quantities provided are 1$\sigma$.}
    \begin{tabular}{c c c c c c}
    \hline
    \textit{XMM Newton} & 0-0.15$R_{500}$ & 0.15 - 0.3 $R_{500}$ & 0.3 - 0.55$R_{500}$ & 0.55 - 0.75$R_{500}$  & 0.75 - 1.0$R_{500}$\\
    \hline
        $Z_{tot}$ ($Z_\odot$)& 0.47 $\pm$ 0.088 & 0.24 $\pm$ 0.079 & 0.32 $\pm$ 0.073 & 0.40 $\pm$ 0.13 & 0.14 $\pm$ 0.13 \\
        $kT$ & 3.46 $\pm$ 0.16 & 3.71 $\pm$ 0.18 & 3.18 $\pm$ 0.15 & 3.01 $\pm$ 0.38 & 2.62 $\pm$ 0.41 \\
        dof & 524 & 588 & 399 & 368 & 418\\
        $chi^2$ & 817 & 903 & 539 & 515 & 547 \\
       \hline
    \textit{Chandra} \\
    \hline
        $Z_{tot}$ ($Z_\odot$)& 0.41 $\pm$ 0.10 & 0.43 $\pm$ 0.06 & 0.32 $\pm$ 0.15 & - & - \\
        $kT$ & 3.30 $\pm$ 0.16 & 4.05 $\pm$ 0.25 & 3.0 $\pm$ 0.82 & - & - \\
        dof & 63 & 33 & 76 & - & - \\
        $chi^2$ & 81 & 49 & 83 & - & - \\
    \hline
    \textit{Weighted Values} \\
    \hline
        $Z_{tot}$ ($Z_\odot$)& 0.44 $\pm$ 0.066 & 0.36 $\pm$ 0.047 & 0.32 $\pm$ 0.065 & - & - \\
        $kT$ & 3.47 $\pm$ 0.10 & 3.82 $\pm$ 0.14 & 3.17 $\pm$ 0.14 & - & - \\
    \end{tabular}
    \label{tab:all_measurements}
\end{table*}

\subsection{kT Radial Trend}

\cite{Khosr2006} studied RXJ1416 using XMM Newton and Chandra observations.
The authors determined a radial deprojected temperature profile for RXJ1416.
We find agreement of the kT values within a 90\% confidence interval for all values with those presented in \cite{Khosr2006}, as shown in Figure \ref{fig:kT_all}.

\begin{figure}
    \centering
    \includegraphics[width=0.9\linewidth]{kt_comparison.png}
    \caption{Comparison of radial kT measurements. We find agreement within 2$\sigma$ of all measurements, which may be accounted for by improvements in calibration since 2006.  Here we reference the \cite{Khosr2006} published values as K06.
    \label{fig:kT_all}}
\end{figure}

To further corroborate our radial kT trend, we compare determined values with published kT trends \citep{Khosr2006, Vik2006, Burns2010, Reiprich2013}.
Figure \ref{fig:kT_profile} shows the resulting radial trends.
We find agreement with the projected temperature model from Equation 9 in \cite{Vik2006}.

\begin{figure}
    \centering
    \includegraphics[width=0.9\linewidth]{temp_profile.png}
    \caption{Plasma temperature radial trend of RXJ1416. We compare our XMM Newton and Chandra measurements to published trends \citep{Vik2006, Burns2010, Reiprich2013}.
    \label{fig:kT_profile}}
\end{figure}

\section{Characterizing the EEP}\label{sec:EEP_quantities}
The observed metal abundance in the halos of rich galaxy clusters cannot be explained by the visible stellar populations.
We adopt the EEP theory to explain the measured over-abundance of metals.
The EEP is theorized to be composed of primarily Population II stars that dominate during the reionization period $\sim 6<z<10$, and supplying the metals to enrich subsequent galaxy clusters.

Domination of the Population II generation supplies a high-z limit to the existence of the EEP, but the lower limit requires further consideration.
The gas must have been enriched before the formation of galaxy clusters ($z \gtrsim 2$) as to supply them with metals.
Simulations by \citet{Biffi2018a} and \citet{Biffi2018b}, show that a flat radial metal distribution in a galaxy indicates that metals escaped their host galaxies around $2 < z < 3$.
We consider a redshift range of $3 < z < 10$ for the existence and calculations of the EEP characteristics.

\cite{Bregman2010} (hereafter \citetalias{Bregman2010}) studied the impact of the EEP based on the relation of $Z_{tot}$ and $M_*/M_{gas}$.
If we assume $M_*/M_{gas}$ to be the controlling factor of cluster properties such as the abundance of the EEP, we can write an expression allowing us to constrain the EEP contribution from known measurable quantities, as expressed in Equation \ref{eq:Z_tot}.

\begin{equation}
\vspace{0.4cm}
Z_{tot} = Z_* + Z_{EEP} = a_1(\frac{M_*}{M_{gas}}) + a_2(\frac{M_{EEP}}{M_{gas}})
    \label{eq:Z_tot}
\end{equation}

Factors $a_1$ and $a_2$ are the metal yield from the visible stars with mass $M_*$, and EEP with mass $M_{EEP}$, respectively.
The contribution of the EEP decreases with increasing $M_*/M_{gas}$.
We use a Markov chain Monte Carlo method to fit this relation to the \citetalias{Bregman2010} data, resulting in a final relationship of $Z_{tot}=(0.37\pm0.01)+(0.13\pm0.17)(M_*/M_{gas})$.
Including the data point for RXJ1416 in the fit from \citetalias{Bregman2010} (Figure \ref{fig:fin_fit}) results in no significant changes to the overall relationship: $Z_{tot}=(0.36\pm0.01)+(0.10 \pm 0.17)(M_*/M_{gas})$.

The total metallicity in the cluster is the sum of $Z_*$ and $Z_{EEP}$.
\cite{Loew2013} derived a relation for the expected ICM enrichment (specifically, the Fe mass returned) from the evolved stellar populations as a function of $f_*/f_{ICM} = M_*/M_{gas}$ as $Z_* = 1.06 (M_*/M_{gas})$.
We adopt this relation for $Z_*$ versus $M_*/M_{gas}$.
The remaining contribution to the metallicity by the EEP is found by subtracting the fit for $Z_*$ from the total fit for $Z_{tot}$ versus $M_*/M_{gas}$: $Z_{EEP}=(0.36\pm0.01)-(0.96\pm0.17)(M_*/M_{gas})$.
We move forward with constraining the EEP population based on this fit.

\begin{figure}
    \centering
    \includegraphics[width=0.9\linewidth]{final_fit.png}
    \caption{Fit components for \citetalias{Bregman2010} data with RXJ1416 data point. The red line shows the fit between $Z_{tot}$ and $M_*/M_{gas}$ with 1$\sigma$ errors, fit $Z_{tot}=(0.36 \pm 0.01)+(0.10 \pm 0.17)(M_*/M_{gas})$, and the green line is the contribution from $Z_*$. The EEP contribution, shown by the blue line, is the difference between the two.}
    \label{fig:fin_fit}
\end{figure}

\subsection{EEP Supernova Rate}\label{sec:sne}

We begin our calculation of the EEP expected SN rate by adopting the metallicity contribution and mass for RXJ1416.
From Figure \ref{fig:fin_fit} we determine the EEP metallicity contribution to be $Z_{EEP} = 0.245 \pm 0.056$ $Z_\odot$ for RXJ1416,

\begin{equation}
\label{eq:mass}
    M(r < {R_\Delta}_c) = \frac{4}{3} \pi R_\Delta^3 \Delta \rho_c
\end{equation}

We use Equation \ref{eq:mass} to determine a gravitational mass within $R_{500}$ of $2.9 (\pm 1.0) \times 10^{14} M_\odot$ from the published gravitational mass of RXJ1416 within $R_{200}$, $3.1 (\pm 1.0) \times 10^{14} M_\odot$ \citep{Cyp2006, Khosr2006}.
Here $R_\Delta$ is the radius of the overdensity, $\Delta$ is the overdensity constant, and $\rho_c$ is the critical density of the universe at the redshift of the object.
We then multiply the gravitating mass within $R_{500}$ by the gas fraction for RXJ1416 (0.13$\pm$0.06) to obtain $M_{g,500} = 3.75(\pm 1.3) \times 10^{13}$ $M_\odot$.
The baryonic mass for RXJ1416 is the addition of the stellar and gas mass, resulting in $M_b = 3.96(\pm1.3)\times 10^{13}$ $M_\odot$.
The baryonic mass multiplied by the fractional value of Fe in the Sun (0.0019) and $Z_{EEP}$ ($0.245 \pm 0.056$ $Z_\odot$) at $M_*/M_{gas} = 0.054$ results in the Fe mass held in baryons, $M_{Fe} = 1.85 (\pm 0.85) \times 10^{10}$ $M_\odot$ \citep{AndGrev1989}.

We consider three types of SN for the creation of Fe in the cluster: SNe Ia, core collapse (CC), and pair-instability (PISN).
SNe Ia and CC produce 0.743 $M_\odot$, and 0.0825 $M_\odot$ on average, respectively, for a standard Salpeter IMF \citep{TNY1986, TNH1996, Kobay2006, Loew2013}.
PISN occur in the most massive stars.
The minimum cutoff of PISN is uncertain, with \cite{Chat2021} reporting a minimum mass of $M > $65 $M_\odot$, and \cite{Morsony2014} and \cite{Heger2002} adopting $140 M_\odot$.
We will adopt a minimum mass of 96 $M_\odot$ as \cite{Woosley2017} found that a PISN of initial mass 96 $M_\odot$ produces 0.045 $M_\odot$ of Fe.
In our assumed IMF from \cite{Loew2013}, 3.4\% of the total population will exist within the high-mass range 95-150 $M_\odot$.
If all of the stars with mass 95-150 $M_\odot$ result in PISN, the relative metal contribution will be 0.6\% of the total Fe production, considering mass intervals of 1-8$M_\odot$ for SNe Ia, 8-95 $M_\odot$ for CC, and 95-150$M_\odot$ for PISN.
The contribution of PISN to the total Fe yield for the IMF considered is insignificant relative to the Ia SNe contribution, thus we limit our continued study to just SNe Ia and CC.
We refer to \cite{Morsony2014} for an expanded discussion of the different IMFs required to produce the observed ICM metal enrichment.

The total metal contribution from Ia and CC can be determined by considering the relative contributions from each type of SNe.
We adopt the same parameters as \cite{Loew2013} for a diet-Salpeter IMF where the relative fraction of Ia SNe is $f_{Ia} \sim 20 \%$.
Assuming the remaining SNe are CC ($\sim 80 \%$), the average Fe contribution from an SNe is $0.215 M_\odot$.
The total number of SNe required to produce $1.85 (\pm 0.85) \times 10^{10} M_\odot$ of Fe is then $8.6 (\pm 3.9) \times 10^{10}$ SNe.

The redshift over which we expect the EEP to have existed is not well constrained, $\sim 3 < z < 10$, equivalent to $1.69$ Gyr.
The expected number of SNe (Ia + CC) in a single galaxy cluster is $50.9 (\pm 23.5)$ SNe yr$^{-1}$.
This can be broken down into the expected total SNe Ia, $10.2 \pm 4.7$ SNe yr$^{-1}$, and CC $40.8 \pm 18.8$ SNe yr$^{-1}$ for a single galaxy cluster over $3 < z < 10$.

Supernovae Ia associated with the EEP may be observable in galaxy clusters today due to this time delay.
The delay-time distribution (DTD) of SNe Ia is best fit by $\sim$t$^{-1}$ (Equation 13 in \cite{Maoz2012}).
We determine a normalization factor to this trend by integrating over time and setting the equation equal to the total number of SNe Ia predicted for RXJ1416.
Figure \ref{fig:sne_rate} shows the calculated SNe Ia DTD for RXJ1416 compared to Equation 13 from \cite{Maoz2012}, determined by observations.
Our predicted SNe Ia trend lies below the trend determined from observations.
It is possible that the high-redshift SNe Ia already observed originated from the EEP, but were not identified.

The trend of SNe Ia as a function of redshift may also provide insight into the star formation rate of the population.
Figure \ref{fig:sne_rate} also demonstrates the differing formation rates of the EEP convolved with the SNe Ia DTD.
A burst of star formation will result in a simple decay proportional to t$^{-1}$.
Any extended periods of star formation such as a constant rate and gaussian distribution will widen the initial part of the power-law DTD.
The next generation of telescopes, such as the James Webb Space Telescope (JWST), is needed to probe deep into space and monitor the SNe Ia rate of protoclusters.
Efforts to determine the observation limit of SNe Ia with the JWST have already been undertaken, with estimates extending to z=4 \citep{Reg2019}.

\begin{figure}
    \centering
    \includegraphics[width=0.9\linewidth]{dtd_new.png}
    \caption{Expected SNe Ia rate modeled by a DTD of $t^{-1.1}$  \citep{Maoz2012}. The blue line shows the expected rate for RXJ1416 since the initial formation of the population at time$=0$. The green and dashed red lines show the effect on the observed SNe Ia rate for a period of constant star formation during z=6-10 (green) and for a Gaussian star formation period during z=6-10.}
    \label{fig:sne_rate}
\end{figure}

\subsection{EEP Yield}\label{sec:a2}
The total halo metallicity $Z_{tot}$ is the sum of the metals produced by the visible stellar populations, $Z_*$ and the EEP, $Z_{EEP}$, Equation \ref{eq:Z_tot}.
Each metallicity contribution can be broken down further into a yield factor, $a$, multiplied by the stellar fraction of the respective population.
For the visible stellar population, this factor is $Z_* = a_1 (M_*/M_{gas})$.
\cite{Loew2013} developed this relation for clusters as $Z_* = 1.06 (M_*/M_{gas})$.

The metallicity contribution from the EEP can be written as $Z_{EEP} = a_2(M_{EEP}/M_{gas})$ where $a_2$ is the metal yield, and $M_{EEP}/M_{gas}$ is the EEP stellar fraction.
The value $a_2$ can be determined by first solving for $M_{EEP}$, the total mass of EEP stars, and using Equation \ref{eq:Z_tot} to solve for $a_2$.

The total mass of the EEP needed to account for $Z_{EEP}$ may be determined by dividing the total number of EEP SNe (CC+Ia) by the number of SNe per star formed ($\eta^{SN}$) (Equation \ref{eq:meep}).
We adopt the same diet-Salpeter IMF considered in \cite{Loew2013} which  derives an $\eta^{SN}$ of 0.01.
The total number of EEP SNe calculated in Section \ref{sec:sne} is $8.6 (\pm 3.9) \times 10^{10}$ SNe.
Dividing the total EEP SNe by $\eta^{SN}$ results in $M_{EEP} = 8.6(\pm 3.9) \times 10^{12}$ $M_\odot$.
For the values relevant to RXJ1416, we derive $a_2 = 1.14 \pm 0.16$.
We note that the uncertainties derived for $a_2$ are based on the assumed values of the SNe fraction ($f_{ia}$, and $f_{CC}$), SNe yields ($y_{ia}$, and $y_{CC}$) and number of SNe formed per star formed ($\eta^{SN}$).
The uncertainty is thus independent of any measured value.
The final equation can be written as $Z_{tot} = 1.06 (M_*/M_{gas}) + 1.14 (M_{EEP}/M_{gas})$, from which $M_{EEP}$ may be found for any system with a measured $M_*$, $M_{gas}$, $Z_{tot}$, and assumed $a_1$ and $a_2$.

\begin{equation}
    M_{EEP} = \frac{SNe (CC+Ia)}{\eta^{SN}}
\label{eq:meep}
\end{equation}

\subsection{Future Improvements of EEP Constraints}\label{sec:improvements}

The relation of $Z_{tot}$ vs $M_*/M_{gas}$ was first studied by \citetalias{Bregman2010} who concluded $Z_{tot} = (0.37 \pm 0.01) + (0.13 \pm 0.17)(M_*/M_{gas})$.
Metallicity and stellar fraction values used to determine this relation were obtained from a variety of sources, likely adding to the scatter.
Since \citetalias{Bregman2010}, more data have been made publicly available and calibration files have been improved.
High-precision work may also be applied to the best (brightest and deeply observed) systems, from which one may identify classes of groups or clusters that are statistically different.

We plan to better constrain the EEP contribution and properties by expanding upon the relation between $Z_{tot}$ and $M_*/M_{gas}$.
Data reduction and analysis techniques developed and tested for object RXJ1416 will be implemented for a survey of 27 galaxy groups and clusters.
These selected sources also have $M_*$ and $M_{gas}$ measurements from a single source \citep{Lagana2013}.
Simulations of uniform $Z_{tot}$ measurements of the 27 groups and clusters show a consistent improvement on the slope error by a factor of 2.5-3.

This reduction in errors propagates to reduced errors on the SNe rate and total population mass of the EEP.
Better constraints on this population will allow for a more confident determination of the existence of EEP in future next-generation observations.

\section{Summary}\label{sec:summary}
High-mass galaxy clusters do not have adequate visible stellar populations to produce the measured halo metallicity.
This is the the missing metal conundrum \citep[e.g.,][]{Loew2013}.
A proposed solution to the metal conundrum is a population of high-mass stars that produced most of metals seen in present-day galaxy clusters, the early enrichment population.
The contribution of the EEP to measured cluster metallicity can be determined by studying the relation between $Z_{tot}$ and $M_*/M_{gas}$ \citepalias{Bregman2010}.
A fraction of the total metal comes from the visible stellar population ($Z_*$), and the remainder comes from the EEP ($Z_{EEP}$).

We improve on the halo metallicity determination of RXJ1416 and break down the total halo metallicity into the contribution from $Z_*$ and $Z_{EEP}$.
Measurement of $Z_{EEP}$ allows for constraints to be imposed on the EEP SNe rate.
The primary calculations are summarized below.
\begin{enumerate}
    \item The RXJ1416 halo metallicity was measured to be $0.303 \pm 0.053$ $Z_\odot$ within $0.3 < R/R_{500} < 0.75$ using archival Chandra and XMM Newton data.

    \item Incorporating the halo metallicity of RXJ1416 to the \citetalias{Bregman2010} $Z_{tot}$ versus $M_*/M_{gas}$ relation confirms but does not change the fit significantly: $Z_{tot} = (0.36 \pm 0.01) + (0.10 \pm 0.17) (M_*/M_{gas})$.

    \item The EEP metallicity weight, $a_2$, is calculated to be $1.14\pm0.16$. We rewrite the equation for $Z_{tot}$ to incorporate the yields of the two contributing stellar populations: $Z_{tot}=Z_*+Z_{EEP}=1.06(M_*/M_{gas})+1.14(M_{EEP}/M_{gas})$.

    \item  The visible stellar population RXJ1416 halo metallicty contribution ($Z_*$) is $0.057 \pm 0.019$ Z$_\odot$, and the EEP contribution ($Z_{EEP}$) is $0.245 \pm 0.056$ Z$_\odot$.

    \item An SNe rate $10.2 \pm 4.7$ Ia SNe yr$^{-1}$ and $40.8 \pm 18.8$ CC SNe yr$^{-1}$ for a single protocluster over the redshift range $3<z<10$ is required to produce $Z_{EEP}$ in RXJ1416.

\end{enumerate}

Future work will improve upon the current fit by extending this analysis to 27 additional galaxy groups and clusters.
This sample has a range of $0.024 - 0.48$ $M_*/M_{gas}$, all obtained from a single source \citep{Lagana2013}.
The methodology described in Section \ref{sec:data} will be used to determine halo metallicities for each $M_*/M_{gas}$ and $Z_{tot}$.
These new halo metallicities will be used to rederive the contribution and characteristics of the EEP, decreasing the error by a factor of $\sim$3.
In addition to further study of the observational data, simulations of large-scale structures are needed that take the EEP into account.
Decreasing the error in this relation propagates a decreased error to the SNe rate from which we may determine the existence of the EEP in next-generation telescope observations.

\textit{Acknowledgements}. We deeply thank Alexey Vikhlinin for his help on the reduction of the spectroscopic Chandra data and derived value comparisons.
We would like to thank Cameron Pratt, Jiangtao Li, Zhijie Qu, Rui Huang, and Hang Yang for thoughtful discussion over the course of this research project.
The authors would like to gratefully acknowledge support for this program through the NASA ADAP award AWD 012791.

redpajama_set_name: RedPajamaArXiv


text:
Washington Memorial for Murdered Muslim Teen Set on Fire
By VOA News, Esha Sarai
Items left at an impromptu memorial in Washington for slain Muslim teen Nabra Hassanen were set on fire, June 21, 2017. (E. Sarai/VOA)
A memorial of flowers and posters made for murdered Muslim teen Nabra Hassanen in Washington was set on fire Wednesday morning.
D.C. park police arrested 24-year-old Jonathan Solomon of North Carolina and charged him with vandalism. Park police have said it is unclear whether the items he set ablaze had been a part of the vigil held for Hassanen the day before or his own items.
Flowers were lain and candles lit in the circle Tuesday night for Hassanen, a 17-year-old from Sterling, Virginia who was beaten to death with a baseball bat on her way to the mosque Sunday night.
An attendee leaves flowers for Nabra Hassanen, a t
An attendee leaves flowers for Nabra Hassanen, a teenage Muslim girl killed by a bat-wielding motorist near a Virginia mosque, during a vigil in New York City, June 20, 2017.
Tuesday night's vigil, which featured local speakers and Muslim activists, was followed by a prayer and iftar - a meal breaking the daily fast Muslim's observe during the month of Ramadan.
Hassanen's killer, 22-year-old Darwin Martinez Torres, was arrested and charged with murder earlier this week.
Hassanen's killing sparked outrage and solidarity on social media, with many activists calling on police to investigate it as a hate crime. Family members say Hassanen and other girls in her group were wearing hijab, Muslim head scarves, when the attack occurred. But police and some witnesses said Torres appeared to be agitated by a traffic argument, not religious hatred.
Rights Activists, Muslims Hold Vigil for Slain Muslim Teen
Young Muslim women joined with women's rights advocates in Washington, D.C. Tuesday evening to mourn a 17-year-old killed in nearby Sterling, Virginia over the weekend.As traffic swirled around DuPont Circle, a small circular park nestled in the center of one of Washington's major boulevards, the diverse crowd listened to activists, poets, and an imam honor Nabra Hassanen and denounce violence toward women, Muslims, and African-Americans. Authorities say Hassanen…
By Esha Sarai
US Muslim Teen Found Dead After Assault Near Virginia Mosque
Police in the eastern U.S. state of Virginia have charged a man with murdering a 17-year-old girl after assaulting her as she walked with friends from a nearby mosque in the suburbs of Washington, but now say they are not investigating it as a hate crime. Authorities said there was a "dispute" early Sunday between the two sides, and that friends of the girl, identified as Nabra Hassanen, fled as he got out of the car to attack her. The…
Esha Sarai

redpajama_set_name: RedPajamaCommonCrawl


text:
Search Properties | About Us | Contacts & Directions | Local Area Services | Home
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40 acre ranch in Dunlap - Excellent land w/ home and a pond
Type: Ranch/Farm (over 10 acres)
City: Dunlap
County: Fresno Bedrooms: 3
Acres: 40 Well: Yes
Septic: Yes
Sqr Feet: 2028
Please call for address
Grade School: Dunlap
Junior High: Dunlap
High School: Reedley
APN: 19008017
MLS: Lot Number:
Track Number: Status: Available
Listings in Dunlap don't come up too often. Here's a rare chance for a 40 acre ranch on Millwood Road. It has excellent land that is fully usable, a ranch style home, and a pond. It also has a lot more going for it. Hands down, this property has some of the nicest land on the mountain!
Location is on Millwood Road, just over a mile from the Dunlap School. The custom home was built in 1977 and features 2,028sqft in a ranch style layout with 3 bedrooms and 2 baths plus a 2 car attached garage. Adjacent to the home is a large barn with electricity, some additional outbuildings, and a well. The 40 acres is fenced into four roughly 10 acre sections. The home and barn are in one section. To the east is a second section with a nice pond and a second well (not presently in service). South of the home is a third section that consists of a home site(w/ old singlewide mobile), second electrical service, septic, and a 3rd well that is presently in use. East of the third section is an additional 10 acres that is separately fenced. All of the property has excellent, very gentle terrain with open pasture areas and a nice coverage of mature oaks. The location is in an area of larger parcels (40 acres and up) where easement roads provide access from Millwood Road.
How about any negatives? This is a court ordered sale that will require approval by the judge. The easement roads segregate the eastern two 10 acre sections from the western two sections and from each other. It's not a big issue as it has little impact on utilizing the land. There is a lot of junk and debris on the property. This is the original owner and they have been dedicated "collectors" during their more than 40 years of ownership. A new roof was installed on the home approximately 5 years ago but the interior of the home does need some work. The home is sound but dated with little maintenance over the last couple of years.
Don't let the negatives keep you from looking at this property. It is an outstanding piece of foothill property that has real potential. It does need a lot of elbow grease but you would be hard put to find a better piece of land anywhere up here. Showings are by appointment only with the listing agent present and a minimum of 24 hours notice.
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text:
September 04: All-Africa Games
What: The 11th African Games
Where: Brazzaville, Congo
When: September 04 - 19, 2015
More: Quadrennial multi-sport event featuring 20 sports, including traditional Olympic events such as athletics and swimming, plus karate and petanque.
Fun Fact: 2015 marks the 50th anniversary of the Games; the first edition was also held in Brazzaville, and featured over 2000 athletes from 29 nations (54 nations expected this year).
Official: http://www.cojabrazzaville2015.com
Tracking the calendar of key international Olympic sport events (World, Continental and Regional Championships, World Cups, etc.) throughout the year.
*(Am I missing something you think should be here? Send me a comment in the 'About' page!)
Favorite Sites
NBC Olympics
Olympic Historian Society
African Championships
Asian Championships
Cross Country Racing
Oceania Championships
Olympic Qualification
One-day Event
South American Championships


text:
Auto Service CUSO Restructures to Cope With Economic Downturn
The downturn in the auto industry has put auto lending CUSO Auto Expert in the position many other companies are finding themselves in these days: how to bring down costs to make up for loss of revenue.
By Lindsey Siegriest | March 10, 2009 at 08:00 PM | The original version of this story was published on Credit Union Times Magazine
The downturn in the auto industry has put auto lending CUSO Auto Expert in the position many other companies are finding themselves in these days: how to bring down costs to make up for loss of revenue.The CUSO has had to conduct some internal restructuring in order to cope with the effect the economy has had on auto sales."Due to the slow down and contraction, we've had to lay people off to bring down cost to make up for loss of revenues," said Auto Expert President Chris Andrus. "We're doing more with less."Auto Expert is a subsidiary of Riverside, Calif.-based Altura Credit Union. The CUSO offers auto-locating services to 20 credit unions.Auto Experts' credit union partners refer members looking for a car to the CUSO and Auto Expert then finds the exact car the member is looking for and schedules the delivery of the car. The service eliminates the process of the member having to deal with a dealership and car salesman.The second half of 2008 was particularly tough on Auto Expert with the economy continuing to slide and the troubles of General Motors, Chrysler and Ford becoming prominent."The overall economy has had a psychological impact on people, which is causing them to sit on the sidelines right now and hold on to a car they might have otherwise turned in for a new car," Andrus said. "The loss of jobs has caused credit scores to go down while at the same time standards for a loan are being raised so some people who want to get a loan can't."Maintaining high services and strong relationships with its credit union partners is a major priority right now for Auto Expert, according to Andrus."The majority of our referrals come from credit union employees, so we want to continue to build focus there and work with loan officers to provide education and incentives."Auto Expert has had 11 new credit union partners come on board in the past two years and had two new partners, El Monte, Calif.-based SCE Federal Credit Union and Chatsworth, Calif.-based Matadors Community Credit Union, join last month.SCE FCU has more than 41,500 members, assets of $413 million, serves employees of Southern California Edison and expanded its membership in 1998 to include other business and underserved communities in Southern California. Matadors CCU has more than 13,000 members, assets of $122 million and serves Cal State University students, alumni, athletic boosters, faculty, staff and anyone who lives works or worships in certain Southern California communities.When developing a program for its credit union partners Auto Expert works with the credit union to create a name for the program so the credit union can market it and members are familiar with it by name."At SCE FCU our private label for this auto buying service is called 'CU at the Wheel.' It offers our members the convenience and peace of mind they can only get from their credit union. A member in the market for new vehicle just has to pick up the phone or stop by one of our branches, and our team of Auto Expert vehicle advisers will do the rest. After negotiating the best possible price, they will deliver the vehicle to the member at a branch or their home or office. And members already know our rates are hard to beat and our service is our passion."For Matadors CCU Vice President of Marketing Marnie Nemcoff said that Auto Experts emphasis on member service and being a quality organization were the key factors the credit union looked at when making the decision to partner with them.Andrus said that he expects they will have more credit union partner's sign on this year, but in the current climate it's hard to say and that's why strengthening the relationships they have with current partners is so important.Auto Expert advisers attend SEG events with the credit union's marketing department. They also attend branch meetings and new employee trainings. The CUSO will donate prizes and participate in raffles a credit union may have to continue to build that relationship."We want to be a part of the credit union culture and we want to earn the referrals we get," Andrus said.With the staff layoffs, Andrus said that another key part to the CUSOs plan this year is to make sure that the staff is in-line with the number of members they have coming in and that advisers are not overwhelmed so they can still offer a high level of member service."We need to stay lean in order to be strong for when things do turn around so we need to hone in and focus on what we do well."Andrus said that the CUSO has a 98% member satisfaction rate and that its net promoter score is 97%. The net promote score gages what members that use Auto Expert's services will recommend it to a friend. Andrus also said that 92% of its services result in a credit union loan.–[email protected]


St George Illawarra skipper Gareth Widdop enjoyed a bumper 2017 season, and was given the chance to reflect on the year that was.
Widdop finished the season as Dragons Player of the Year and he also won the RLPA and Dally M Five-eighth of the Year.
Finishing third on the overall Dally M Leaderboard, Widdop would've also played in England's mid-season Test against Samoa if not for a knee injury suffered on Anzac Day.


text:
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namespace Cerad\Bundle\GameBundle;

use Symfony\Component\HttpKernel\Bundle\Bundle;

use Cerad\Bundle\GameBundle\DependencyInjection\GameExtension;

class CeradGameBundle extends Bundle
{
    public function getContainerExtension()
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redpajama_set_name: RedPajamaGithub


text:
Tag: Sweetness and Lightning
Summer 2016 Anime First Impressions
written by Laurie Tom
There's a lot of good stuff this summer, so much that I'm glad my plate is currently clean of other series because I may end up watching a bit more than usual.
Why I Watched It: Original mafia TV series set in the Prohibition era? Sign me up. The story is to take place over 91 days during which the protagonist returns to his old stomping grounds to exact revenge for the murder of his family.
What I Thought: I hadn't expected that Angelo was only a kid when his parents and brother are killed in a change of power in the mafia family his father belonged to, and he grows into a teenager under the new name Avilo Bruno to hide his real identity. Despite his age, Angelo is fairly hard bitten and we don't see the entirety of his plan in the first episode, but it looks like his goal is to infiltrate the Vanetti Family, because it will easier to exact revenge when his target thinks he's a trusted comrade. What we do get is some bootlegging, a violent encounter with the powerful Ocro Family, which leads into Angelo and his friend Corteo meeting up with Nero Vanetti, who was one of the men responsible for killing Angelo's family.
Verdict: I'll be watching! Though the setting looks more European than East Coast, the show strikes the period mood it goes for with its reserved color palette and brutal gang wars. Also worth mentioning is that Corteo is a PoC, which is rare for a mafia drama. Angelo probably isn't a protagonist people are going to relate to, but the guy's got guts, so he'll probably be fun to watch.
Where to find stream: Crunchyroll
Why I Watched It: Berserk is not my normal cup of tea. I dislike grimdark fantasy in general, and the series is known to have a way with mentally and physically breaking its characters. But I got to know the protagonist, Guts, before I knew all that, while watching my brother play one of the Berserk video games, so I'm more inclined to give this a shot.
What I Thought: Though the anime is not starting at the beginning of the manga, I feel like the opening episode establishes all that really needs to be known about Guts before jumping in. He's cursed, some bad mojo went down in his past, and it's a really bad idea for anyone decent to hang around him because they're probably going to get killed. The animation is a little janky with the obviously computer animated enemies versus the 2D appearing Guts, but considering the world itself doesn't seem quite right, that's probably okay. A group of bandits get eaten by forest demons before they even get close to getting revenge on Guts, so this is clearly a messed up place to be. Guts himself is a little ridiculous when it comes to combat ability, there's even a narrator explaining how his sword is too big to realistically be considered a weapon, but the character's no nonsense approach to everything he does sells it.
Verdict: If this was another season, I'd be watching, but there's just too much this time around. Berserk has been one of the classics I've heard about for years, and this is not its first time being animated, but this is the first time this particular story arc has been.
D. Gray-man Hallow
Why I Watched It: D. Gray-man was one of last long-running shounen series I watched, because I liked the characters and the macabre worldbuilding. If the bereaved want to bring a loved one back to life, it's entirely possible, though the price is incredibly high. The resurrected become akuma, monsters devoted to the service of the malevolent Millennium Earl. The original series ran for 103 episodes in 2006-2008, but only half have made it to the US. In the wake of Hallow the second half has been licensed since Hallow continues the manga storyline from where the earlier series left off.
What I Thought: Can you catch up? Is it worth it? It's possible to get a feel for how the story has progressed if one is familiar with the earlier licensed portion of the anime, but even with that grounding, it's obvious that a lot of time has passed and some serious business has gone down. The exorcists of the Black Order look older, more battle worn, and protagonist Allen Walker is now host to the memories of someone who could be considered one of the bad guys. I wouldn't recommend jumping in without at least some familiarity with the series, otherwise a lot of what happens in this first episode will have no weight, and there's a lot that clearly does.
Verdict: I'm going to pass. Though I like seeing all the familiar faces again, it's clear that I missed a huge turning point in the battle with the Earl which was probably the climax of the previous series. Now that I know the rest of the original has been licensed, I'll wait for that to come out and watch Hallow afterwards.
Where to find stream: Funimation
Danganronpa 3: The End of Hope's Peak Academy – Future
Why I Watched It: This is the conclusion to the storyline started by the Danganronpa video games and not actually based on a game itself. Because of gameplay constraints (which players will understand) it would have been difficult to provide a proper send-off to the Danganronpa 1 cast without stretching believability. This anime is supposed to do that and conclude the Hope's Peak Academy storyline.
What I Thought: I was a little concerned by how large the cast is jumping in, but it's aided by the fact there are a number of returning characters who survived the first killing game. People who have only watched the first anime and not played Danganronpa 2 are guaranteed to be lost though, as the second game was never animated and the two minute recap doesn't even begin to cover what happened, but fans of both games can comfortably jump in. Oddly enough, two of the characters who ought to be returning, Byakuya and Toko, are nowhere to be seen, but hopefully they'll have cameos later. The first episode is well paced, getting Makoto Naegi accused of treason for his actions in Danganronpa 2 as well as bringing back series villain Monokuma, who starts things off with a bang. Nothing like a murder to begin the next killing game!
Verdict: I'll be watching. Danganronpa has a reputation for being dark with a black sense of humor, and it's all there. Even the opening credits are fairly messed up, depicting the potentially gruesome deaths for each cast member, so the audience has no idea who will survive (though I think Makoto will make it). The writer for the Danganronpa games laid out the story for the anime-only conclusion so this is as canon as it gets.
Danganronpa 3: The End of Hope's Peak Academy – Despair
Why I Watched It: Though it's airing in the same season, Despair is a separate show with its own opening/ending credits sequence from Danganronpa 3: The End of Hope's Peak Academy – Future. This is a prequel to Danganronpa 2 and follows the story of the DR2 cast leading up the start of the game.
What I Thought: Being animated at the same time as the Future arc there is some crossover with the new characters, which I'm fine with since it's helping to implant them in my memories, but unlike Future which begins and remains dark, the Despair arc's first episode is mostly comedic and focuses on getting to know the students of Class 77 rather than any sort of plot. Given what's to come (the arc is named Despair for a reason), I'm pretty sure that's intentional since the mood is all downhill from here. Though it's not possible to be spoiled from the first episode, if the story goes all or even most of the way to the start of Danganronpa 2 it will spoil one of the end game twists for anyone who hasn't played it.
Verdict: I'll probably be watching, but mostly because I'll already be watching Future. Since this is a prequel I already know where they're going to end up, it's more of a question of how they get there and whether or not I want to watch something that's likely to be a horrible downer. It's worth noting that in Japan the Future arc airs before Despair and it's possible Despair will spoil things in the former even though they take place in different time periods.
Why I Watched It: I liked the premise, that a high school girl receives a mysterious letter from herself ten years in the future, telling her that a new student is coming to her school and that she should watch him. The manga has been on my periphery for a while, so I'm looking forward to seeing what people like about it so much.
What I Thought: This series is likely to become a tearjerker due to the kicker at the end of the first episode when sixteen year old Naho Takamiya gets to the end of the letter she receives from her future self. Though there are a couple scenes in the future, most of the story takes place in the past with teenage Naho gradually reading through the letter and parsing the things her future self tells herself to do (or not do) in order to avoid her biggest regrets. Meanwhile, Naho and her friends adopt the transfer student, Kakeru, surprisingly fast, but it gets everyone introduced quickly and none of them feel like stock characters. The sequence of the six of them screwing around in the park was a lot of fun. Though there is a science fiction premise in the existence of the letter, the story itself plays more like a high school drama.
Verdict: I'll be watching! The ending definitely sets up the stakes and will make the days to come more meaningful to Naho, but I wonder if things could potentially backfire from what her future self intended.
Why I Watched It: I love the manga, where unemployed 27-year-old Arata Kaizaki takes part in an experiment to relive a year of life as a high schooler and see if he can come out of the experience with the skills necessary to fix his life as an adult (primarily, getting a full time job). The manga is great at juxtaposing the physically teenage Arata's behavior with his chronological age as he has the perspective from having been an adult for several years, while also being completely terrible at schoolwork because he's forgotten everything.
What I Thought: I think I laughed harder at the manga, but it translated surprisingly well to the screen considering it's mostly a series of short scenes about Arata getting into awkward situations. This time there's a bonus for those with some understanding of spoken Japanese since fish-out-of-water Arata speaks like an adult among strangers rather than a student among classmates. While the premise is similar to Orange along the lines of re-doing high school for fewer regrets, this is more of a comedic take with golden moments like Arata unwittingly bringing cigarettes to class without thinking about why that would be a bad idea.
Verdict: I'd like to watch, but given how crowded this season is, I'm not sure. I would highly recommend it for those who haven't already read the manga, but the humor doesn't seem to be quite as effective a second time around so it's a little lower on my priority list. The episodes for this one are being posted extremely quickly rather than the usual once a week schedule, so there will likely be a full season's worth by the time this article is posted.
Sweetness and Lightning
Why I Watched It: Slice of life isn't entirely my thing, but I figured I'd give it a shot since this series involves a single dad raising a young daughter, and having been raised by a single dad this piques my curiosity. Interestingly, the original manga ran in a magazine for young adult men.
What I Thought: It's definitely sweet, as Tsumugi is adorable and unusually compliant for a kindergartner. Her father Kohei is also extremely patient for a recent widower. Their family life at the start of the story feels a little too romanticized for being only six months after their loss, but that said, Kohei's struggle to properly care, and especially cook, for his daughter rings true. We see him pass on hanging out with coworkers after work because he needs to go home to her, and him picking up prepackaged meals because he can't cook. There's no doubt he cares about her, but he's not really prepared to be a single father. The only beat that feels off is the introduction of one of his students who looks to become a regular character, because I have trouble with a high school girl hanging out with her teacher outside of school.
Verdict: I'll probably pass on account of this not being my thing, but it's delightful to see a series squarely aimed at adults and what it's like being a single dad of a very young child.
Laurie Tom is a fantasy and science fiction writer based in southern California. Since she was a kid she has considered books, video games, and anime in roughly equal portions to be her primary source of entertainment. Laurie is a previous grand prize winner of Writers of the Future and since then her work has been published in Galaxy's Edge, Strange Horizons, and the Year's Best YA Speculative Fiction.
Posted on August 19, 2016 August 8, 2016 Author Laurie TomCategories ReviewsTags 91 Days, anime, Berserk, D.Gray-man Hallow, Danganronpa 3: The End of Hope's Peak Academy, Laurie Tom, Orange, ReLIFE, Sweetness and Lightning2 Comments on Summer 2016 Anime First Impressions


Copyright © Janice G. Fischel. All rights reserved.
Behind the camera I am a native of Bethlehem, Pennsylvania, and a graduate of Moravian College. I have lived in Hanover, New Hampshire, since 1973. My family and I have spent several years on the west coast, having lived in Davis, Berkeley, and Santa Barbara, and in Seattle, on sabbaticals from Dartmouth College where my husband teaches economics.
Though I have had an interesting array of jobs over the years, I have consistently taken photos everywhere we have been. I am always delighted to find an uncommon view of everyday things.


text:
Q: Node.js Asynchronous Callback Function Not Working As Reqiured I am trying to design a registration page in node.js using Knex.js and mysql.
Here is the code:
Registration Page
`
router.post('/', function(req, res, next){
    var fname = req.body.fname;
    var mname = req.body.mname;
    var lname = req.body.lname;
    var email = req.body.email;
    var uname = req.body.uname;
    var pwd = req.body.password;
    var conf_pwd = req.body.conf_password;
    var tnc = req.body.tnc;
    var errors = req.validationErrors();

    //Validation
    req.checkBody('fname', 'The First Name is Required').notEmpty();
    req.checkBody('mname', 'The Middle Name is Required').notEmpty();
    req.checkBody('lname', 'The Last Name is Required').notEmpty();
    req.checkBody('uname', 'The Username is Required').notEmpty();
    req.checkBody('email', 'The Email is Required').notEmpty();

    var rand = Math.floor(Math.random()*90000) + 10000;

    //hash The password
    var hashpassword = crypto.createHash('sha512').update(pwd).digest('hex');
    var IdVal = email+uname;
    var IdHash = crypto.createHash('sha512').update(IdVal).digest('hex');
    var tstamp = new Date().toString();
    //Add The User
    if(errors){
        res.render('register', {
            errors: errors
        });
    }else{

        var newUser = ({
            Id: IdHash,
            FirstName: fname,
            MiddleName: mname,
            LastName: lname,
            Email: email,
            UserName: uname,
            HashPassword: hashpassword,
            ActivationCode: rand.toString(),
            ActivationStatus : false,
        });
        User.CheckUser(uname, function(stat){
            console.log('Stat : ',stat);
            if(stat == 1){
                res.render('register', {
                    uerrors: "The Username Already Exists"
                    });
            }else if(stat == 2)
            {
                res.render('register', {
                    uerrors: "Error Occured"
                    });
            }
            else if(stat == 0){
                User.CreateUser(newUser, function(err){
                    if (err){ throw err}
                    else{
                        res.render('register', {
                            message: "Verification Email Sent Please Check Email"
                        });
                    }
                });
            }
        });
    }
});

So What i Wanted to do is check if username exists. If not then create the new user and then show that user is created. And Here is the Code in User.js
module.exports.CheckUser  = function(uname, callback){
    knex('Clients')
        .where({UserName: uname})
        .select()
        .then(function(result){
            if(!result || !result[0]){
                console.log('User Not Found');
                callback(0);
            }else{
                if(result[0].UserName == uname){
                    callback(1);
                }
            }
        })
        .catch(function (err){
            console.log(err);
            callback(2);
        });
}
module.exports.CreateUser = function(newUser, callback){
    knex('Clients')
        .insert(newUser)
        .catch(function (err){
            callback(err);
        });
}

Here, what exactly is happening that the functions in user.js are getting executed first and then it is showing that the username already exists. But the username is just created.
Here is the output of the code,
GET /register 304 670.944 ms - -
GET /bootstrap/css/bootstrap.min.css 304 9.677 ms - -
GET /dist/css/AdminLTE.min.css 304 7.780 ms - -
GET /plugins/iCheck/square/blue.css 304 7.291 ms - -
GET /plugins/jQuery/jQuery-2.2.0.min.js 304 2.312 ms - -
GET /bootstrap/js/bootstrap.min.js 304 2.259 ms - -
GET /plugins/iCheck/icheck.min.js 304 2.076 ms - -
GET /bootstrap/fonts/glyphicons-halflings-regular.woff2 304 0.468 ms - -
GET /plugins/iCheck/square/blue.png 304 0.439 ms - -
{ method: 'select',
  options: {},
  timeout: false,
  cancelOnTimeout: false,
  bindings: [ 'q' ],
  __knexQueryUid: '99707783-2767-4c37-ae4c-0bd31f98427d',
  sql: 'select * from `Clients` where `UserName` = ?' }
User Not Found
Stat :  0
{ method: 'insert',
  options: {},
  timeout: false,
  cancelOnTimeout: false,
  bindings:
   [ '41040',
     false,
     'ameya.pandya@securelayer7.net',
     'q',
     '2e96772232487fb3a058d58f2c310023e07e4017c94d56cc5fae4b54b44605f42a75b0b1f358991f8c6cbe9b68b64e5b2a09d0ad23fcac07ee9a9198a745e1d5',
     '70b32fc5adc4d2fa6ad5a40d9b6bfe4acc745d0c9c71d47a8266a4d54868198acb29644dc6133fb51cd682dcf1fc72a52278a51ade397ed7f2a38f8ec809e0bf',
     'q',
     'q',
     'q' ],
  __knexQueryUid: 'dee0340f-c247-4608-a29e-da984cc13e49',
  sql: 'insert into `Clients` (`ActivationCode`, `ActivationStatus`, `Email`, `FirstName`, `HashPassword`, `Id`, `LastName`, `MiddleName`, `UserName`) values (?, ?, ?, ?, ?, ?, ?, ?, ?)' }
POST /register - - ms - -
{ method: 'select',
  options: {},
  timeout: false,
  cancelOnTimeout: false,
  bindings: [ 'q' ],
  __knexQueryUid: 'a58fe912-3a9e-4af0-85ca-e1ba2aa9559b',
  sql: 'select * from `Clients` where `UserName` = ?' }
Stat :  1
POST /register 200 105.596 ms - 3234

A: Your output shows that the user does not exist. CheckUser prints 'User Not Found' and calls callback(0). stat equals 0 which is why a new user is created by the following code.
else if(stat == 0){
   User.CreateUser(newUser, function(err){
     if (err){ throw err}
       else{
         res.render('register', {
           message: "Verification Email Sent Please Check Email"
         });
       }
     });
}

redpajama_set_name: RedPajamaStackExchange


text:
JAGMOHAN SINGH | November 13, 2018 05:04 PM
AMRITSAR: Former four times MLA, former Punjab Cabinet Minister, Gobind Singh Longowal becomes 43rd Shriomani Gurdwara Pharbandhak Committee (SGPC) President during its annual general house meeting. He was re-elected today as first time he became President of this prestigious religious body last year November 2017.
His name was first proposed by the former SGPC President Bibi Jagir Kaur thereafter another former SGPC president Avtar Singh Makkar seconded his name.
Longowal was the sole candidate for post of SGPC president when his name was proposed by Bibi Jagir Kaur as none of the SGPC came forward to contest against the serving president. Hence he was elected unanimously amidst the religious slogans of Bol-e-So-Nihal Sat-Sri-Akal at the mini Sikh Parliament in Teja Singh Samudari Hall in the SGPC premises.
However, Gurbachan Singh Karmuwal elected as General Secretary as Ragujit Singh Virk has been elected as Senior Vice President of SGPC. Similarly Bikar Singh was elected as junior vice president of SGPC.
Gobind Singh Longowal who becomes the SGPC chief remained MLA in 1985, 1997 and 2002. He had also win by-elections from Dhuri when Congress MLA Arvind Khanna resigned in 2015. Longowal was also remained cabinet minister in the Akali Government. He had become SGPC member in 2011.
However, eleven Executive members were also elected are Amrik Singh, Gurmit Singh, Bhupinder Singh, Jarnail Singh, Jagjit Singh, Kushwinder Singh, Manjit Singh, Amrik Singh, Jasbir Singh, Shingara Singh Lohian and Tara Singh.
Some SGPC members boycotted the elections when the name of Gobind Singh Longowal was proposed. They left the venue by saying that they were supporting the Sikh people staging stir at Bargari demanding arrest of culprits accountable for sacrilege of Guru Granth Sahib.
It may be added here that there are total 180 members of SGPC General house out of which 174 members have right to vote, whereas 159 elected and 15 are nominated.
There was much chaos when female SGPC member Bibi Kiranjot Kaur stood to speak to defend the historian Dr. Kirpal Singh. She was not allowed by the SGPC members to speak on the dais and bedlam remained continued unless she left.
Agitating SGPC members were saying that Dr. Kirpal Singh was instrumental for preparing the Sikh history text books of PSEB. Keeping in view the gross distortion of facts in the 12th standards text books SGPC had recently decided to disassociate with Professor Kirpal Singh.
Chhath Puja: Vendors doing brisk business as mango wood, bamboo baskets in high demand


I love this rainbow bright top!
It was the first item I selected & then had to play the LBB game to get other items I wanted!
I love when a Little Black Bag arrives!
Also loving thèse Deux Lux bags!
With promo these amazing items only cost me $10!


text:
Episode 94 - Old Bobby Fartypants (Showmen Week)
Tom's Notes: Joseph Pujol
I started this week's research committing myself fully to a chap called Edward Kelley. I thought to myself, this guy's story is going to funny and fascinating. Then I began to read some of his works from the 16th century, and I realised that I could not be arsed. Let me now discuss him as an honorary mention.
Edward Kelley was a Welshmen who lived during the second half of the 16th century. He fits into the theme of showmen because he was a complete charlatan who made a living spouting shite to dumb posh people. Well at least that's how history remembers him - I could easily believe that his intentions were genuine. He's a great example of the Dunning-Kruger effect.
He was basically an alchemist who devoted his life to making base metals into gold. Something he wasn't very good at. Now I wanted to go straight for his work, which is easily accessed online, and things started promisingly. One chapter of his is called The Humid Way, or a Discourse on the Vegetable Menstruum of Saturn. This chapter heading is doubly amusing and surreal when one assumes that the word menstruum refers to a lady's time of the month. Do vegetables menstruate? one might shout from the back of the audience. Do vegetables exist on Saturn another eager listener might question. Well, fools, menstruum is an archaic word for a solvent. Now when you re-read the title, it makes much more sense, listen, The Humid Way, or a Discourse on the Vegetable Solvent of Saturn. Oh, that makes much more sense.
I still sense Sam that you are thinking, this is gold, well, almost gold, what could possibly go wrong with this source? Well, let me quote part of it and then we can all agree that this is total nonsense that Tom cannot be arsed trying to wade through to find fart jokes and French accents.
Of these elements two, viz., fire and water, are active, while two, earth and air, are passive. Fire and water strive to unite them- selves to earth, but can do so only by means of the qualities which they have in common with it, i.e., in the case of fire, dryness, and, in the case^ of water, coldness. So fire and water introduce themselves into earth by means of their dryness and coldness, ' and into air by means of their heat and moisture. Now, according as earth is more or less dry or cold, its centre will be occupied either by fire or water, while the other active element will be confined to its circumference. In the former case, the inborn dryness or heat of the fire being invisible and intangible, and residing, as it were, at the heart of the earth, will escape obser- vation, but the humidity of the water, being more tangible and nearer to the surface, will be more easily noticed. '1'he surface of this compound will thus be watery, cold, and dry ; and such is the substance which is commonly called quicksilver.
So anyway, that's Edward Kelley for you, nutcase alchemist. Incomprehensible garbler.
Having been disappointed by Edward Kelley. I decided to about turn and go somewhere where fart jokes and French accents are abundant, Joseph Pujol, a man who headlined the Moulin Rouge in the late 19th century and pulled bigger crowds than the famous stage performer Sarah Bernhardt. A charismatic and suave Frenchman from Marseille with coiffured hair and a regal moustache. A man who was always dressed very smartly. A dignified man.
So what was Pujol's act I hear you cry? Well his stage name was Le Petomane, which translates roughly as Fartomanic. Yes, he was a flatulist!
He was a fartomaniac
He would play flutes out of his ass
He could fart on demand
In time with brass bands
He was fartomain-ee
Anally insaney
Fartomaniac!
Those are all facts.
As the story has it, Pujol discovered he have a cavernous, breathing arsehole when as a child he went for a swim in the sea and felt a rather cold sensation in his abdomen. He rushed ashore, confused by what was going on, and then managed to release a few litres of salt water from his bottom. And so greatness was born.
His trick was that he could inhale air into his arsehole and expel it on demand. He didn't have the digestive system of a cow. Early on in his life this 'talent' (and I have written that word in inverted commas in my notes) was something he showed his chums in the army. You know, blokes sitting around in the mess, talking arseholes. It's was real men do. You know, sucking 2 litres of a water into your arse and then squirting it across the canteen. Man fun.
A little later he became a baker where his talent impressed and amused customers. I'll be honest, not for me. I'd rather just have me baguette and be off. I don't want someone parping La Marseillaise with a twinkle in his eye. It's worth pointing out at this point that I painted a picture of Pujol as a smart and charismatic man. I sort of exaggerated this for comic effect. He did indeed perform on stage in a smart outfit, presumably because it was funny juxtaposed with him farting, but I have seen a few pictures of him where he looks like a cross between Office Crabtree and Eric Cantona. Interestingly, if you watch that footage of Cantona kicking a Crystal Palace fan with the volume up, you can here Cantona farting frère Jacque. He is a rather creepy looking mono-browed man who I wouldn't want baguettes off regardless of his bowel hobbies.
When Pujol realised that he was sitting on a rear that could make him millions, he hired a stage in Marseille and started strutting his guff. Much like a stand-up today would go along to an open mic night. Oh and boy did Pujol take off, not literally, he was good but not that good. News spread like the buttocks of a French flatulist and before long, he was selling out venues.
Pujol decided that the next step was gay Paris. He got in touch with the man who ran the Moulin Rouge, a chap called Charles Zidler. Imagine the audition. "What's your act boyo, (yes, this a Frenchmen with a Chicago accent who enjoys Welsh colloquialisms)", "Well, you see, I can fart on demand." "I don't believe it, it's impossible! And besides, the stench, it would be horrendous, I won't, I can't…" "FART voulez vous coucher avec moi". "God damn! Your headlining tonight! Popty ping."
So what could Pujol actually do? What was his act?
Well, he did farty impressions. He impersonated a lady on her wedding night, a mother in law, cannon fire, famous people and animals.
He blew out candles, he smoked cigarettes, he played the ocarina and had the audience sing along. He also farted in time with songs.
He could apparently make sounds like letters of the alphabet. He really worked hard on his art this guy!
He really was a hit and performed throughout the world. There is rumour that nurses had to be stationed in the aisles because women in corsets laughed so hard that they feinted.
His appeal was obviously in the fact that farts are inherently funny, but more specifically, his audience were middle to upper class Parisians and what he was doing was ridiculously coarse and shocking. It's the same juxtaposition as mentioned earlier. Man farts in a classy establishment for the rich. I read some articles by academics totally overanalysing why he was so popular and one thing that is stressed is the class-based humour. I'll be honest, making a loud fart and pretending it's a mother in law doesn't sound particularly nuanced to me.
He had some very famous people watch his show too, including that notoriously funny King Leopold II of Belgium. You know the problem with the Congolese, they just don't get a good joke do they? Interestingly, the phrase, 'crimes against humanity' was apparently coined by an American chap called George Washington Williams in a pamphlet in 1890 condemning Leopold's behaviour in the Congo Free State (just another joke from old Leopold).
Things turned a bit sour with the Moulin Rouge at the end of the 19th Century when firstly the Moulin Rouge sued Puyol for establishing his own theatre company and parping over there. Secondly, Puyol sued the Moulin Rouge for replacing him with lady farter who was a complete fraud and used bellows.
At the start of the First World War, the curtains fell on Puyol's arse, and he retired to run a bakery again. After the war he expressed an interest in returning to the halcyon days, but he felt that French humour had changed. He continued to maintain his anus habits, namely regular enemas (during his show career, he did this prior to shows so that the theatre didn't become too fusty).
A short film was made about him in 1979 starring Leonard Rossiter, an old English comedy actor. There's been a best-selling book about him. A character is named after him in Blazing Saddles (the dumb mayor) and he apparently makes a very fleeting appearance in the film Moulin Rouge.


text:
Seth Ennis may have been raised a proud Georgia boy, but the young singer-songwriter is as worldly as the most seasoned traveler — and it shows in his eclectic brand of country music, a sound inspired by his hero Vince Gill, the pop-punk bands he followed each year on the Vans Warped Tour and smooth R&B stars like Usher.
Despite being just 23 years old, the multi-instrumentalist (he's a natural-born drummer) has experienced a lot of life. Seth spent his formative years on a military base in Japan, cut his teeth as a touring musician while living in Raleigh and commuting to Nashville, and has now put down roots in Music City, where through perseverance and a dedication to his craft he landed a record deal with Sony Music Nashville.
As he likes to tell it, it was a case of being in the right place at the right time — and having the raw talent to stand out. "There was a battle of the bands competition here in Nashville and when one of the bands dropped out, I got the call," Seth says. "I called my players together and we killed it." With the victory, Seth secured a coveted performance spot at CMA Music Festival and caught the eye of Sony, as well as one of the competition's judges, producer Corey Crowder. Crowder is now in the studio with Seth, both of them co-producing Seth's debut album.
With the progressive musical risks of current pop music, the finesse of traditional country, strong R&B influences, and a healthy respect for organic sounds (he is a bluegrass fanatic), Seth's music is poised to establish him as a fresh new voice in the genre, one with a rare global worldview.
"Country music is not that big in Japan," he admits with a laugh while describing his type of music. "If I were raised in Georgia my whole life, I'd probably sound a lot different than I do. But because of how much I moved around, and all the cultures I experienced, my sound is especially diverse."
It's one that will fit right in on country music's evolving landscape, where production has become just as key as songwriting. Fortunately, Seth excels at both.
"Production is so important to me, and I like to think I have an ear for it. I'm really picky," he says. "And songwriting is something I've gotten better at since moving to Nashville and learning from great writers like Ben Hayslip and Rhett Akins. The best song always wins, even if it's not my own. I have incredible respect for the writing community."
For his debut single "Woke Up in Nashville," Seth wrote with tunesmiths David Hodges and Blair Daly, creating an autobiographical account of his journey to Music City to pursue his dream as a singer-songwriter.
Fittingly, the song begins with Seth loading up his father's truck and driving north from Georgia. In the studio, Seth played every instrument on "Woke Up in Nashville," from guitars and bass to drums and piano. He even sang his own background vocals.
Being self-sufficient in the writing room and in the booth is important to the young singer, but he's excited to collaborate in the encouraging country community. Seth is adamant about maintaining his own sense of identity. While he may unabashedly profess a love for pop melody and rock & roll energy, he's a country disciple.
"Country is how I was raised. Its stories are about me," he says. "But Nashville is also a melting pot right now, so I'm thinking huge: What can I do to play internationally? How can I have my songs heard globally? It's about dreaming big."
Which has certainly steered him right so far.
Visit www.OnGuardOnline.gov for social networking safety tips for parents and youth


Click on the ooVoo menu > Settings > Video Messages.
Check "When I log in, send messages from my Outbox automatically".
Click on the Save button to validate.
Published by jak58. Latest update on June 4, 2012 at 06:51 AM by jak58.
This document, titled "ooVoo - Automatically send pending video message on log-in," is available under the Creative Commons license. Any copy, reuse, or modification of the content should be sufficiently credited to CCM (https://ccm.net/).


Image Title: New York Soho Brick Look Porcelain Tile 4 X 8 100086917 Floor For Prepare 14. Filename: new-york-soho-brick-look-porcelain-tile-4-x-8-100086917-floor-for-prepare-14.jpg. Image Dimension: 500 x 500 pixels. Images Format: jpg/jpeg. Publisher/Author: Fermin Considine. Uploaded Date: Saturday - June 16th. 2018 18:55:17 PM. Category: Architecture. Image Source: contemporist.com.
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About 15,000 teachers from three South Western states working under a Federal Teachers' Scheme yesterday protested in Ibadan over non-payment of their salaries by the Universal Basic Education Commission, UBEC.
The teachers, led by Miss Lawal Bukola and Mr. Obayomi Gideon complained that the commission is owing them about N2. 6 billion.
They marched through Dugbe, Agodi Gate and later came to the State Secretariat of the Correspondents' Chapel, NUJ, Mokola roundabout, displaying placards with various inscriptions pleading with the commission to pay the backlog of salary arrears.


text:
Dubai's JLT will be the first area in the UAE to get 5G
Lauren Fletcher
The advanced cellular network is set to make data connection in the district more seamless…
If you live in Jumeirah Lakes Towers (JLT), expect an increase in your streaming or downloading speed this week, as the area will be the first in the UAE to benefit from 5G.
The announcement was made on Sunday October 27 by Dubai-based mobile communications operator, Etisalat and Dubai Multi Commodities Centre (DMCC), with the new network expected to be rolled out some time this week. Yay.
Why JLT? Well, because it's one of the most popular in Dubai for residents and visitors, drawing in over 100,000 people every day. It's a bustling hub of cute little cafes, indie restaurants and gyms that run along by the lakes, so whether people are bedding down to work remotely or catch up with friends, the new high-speed network will no doubt make things even easier.
ALSO READ: When is the next public holiday in the UAE? Here's a guide…
As well as improving the speed of communications and downloads, the new network also looks set to be more economically and environmentally conscious, with smart solution technology that will monitor street lights, parking, noise pollution and environmental changes in the area.
Salvador Anglada, Group Chief Business Officer at Etisalat said "This will transform the JLT community to become the first 5G powered smart district in the region, making it a more seamless, efficient and safe experience for its members, residents and visitors."
No strangers to being leaders of innovation, the UAE won the title of being the country with the fastest home internet in the entire Middle East region, earlier on this year.
It's expected more of Dubai's popular regions will have the 5G network rolled out before the end of the year, so watch this space.
— For the best of Dubai straight to your inbox, sign up for our newsletter.
Images: Supplied


Alisa is a 925 sterling silver ring with a rhodium finishing.
Bea is a ring made of 925 sterling silver with a rhodium finishing.
The Byron Ring is a 925 sterling silver ring with a rhodium finishing.
The Carissa Ring is a 925 sterling silver ring with a rhodium finishing.
Cleo is a 925 sterling silver ring with a rhodium finishing.
Edda is a ring made of 925 sterling silver with a rhodium finishing.
Alanna is a ring made of 925 sterling silver with a rhodium finish.
Lances is a 925 sterling silver ring with a rhodium finishing.
The Waves Ring is a ring made of 925 sterling silver with rhodium finishing.


When it comes to caring for your face, try using gentle pore cleansers and scrubs.
In fact, facial cleanser will also help to improve the circulation of your face. Improved blood flow means a more youthful, line free look.
After all, the goal is to support vital and healthy skin – so feed your skin the nourishing ingredients it needs.
The key to healthier looking skin is to prevent bacteria, oil and dirt from filtering into your pores on a daily basis.
Washing your face at night is an important routine that can prevent blemishes and aging skin.
Using gentle face cleansers to on your face will normalize your skin condition by dissolving dirt and oil on the surface of the skin.
The oil in cleansing face wash is used to dissolve the bad kind of oil on your face. Instead of leaving your face dried out after a wash, replenishing oil penetrates your skin and revitalizes it.
Sufactants dissolves and neutralizes the dirt and grime that is clogged deep down in your pores.
If you use a face cleanser that is too rich for your skin you will work against it. Clogging your pores with heavy cold creams creates a breeding ground for acne.
Likewise, harsh chemical face washes can irritate delicate skin, leaving it dry and sore.
It is important to clean your face thoroughly at night, especially if you wear makeup.
Removing your makeup every night before bed will allow your pores to open up and breathe, in its natural state.
Natural and healthy skin requires pore cleansers for deep and targeted prevention of facial blemishes.
Cleanse your face with warm water to loosen clogged pores and stimulates blood circulation to the skin.
Be sure to rinse with cool water to tighten your pores, water that is too hot or too cold can cause broken capillaries.
Using facial cleansers and scrubs regularly can make a huge difference in your appearance. Keep your skin healthy looking with natural facial cleansers.
Ellen CruzHello! I'm a cosmetic and beauty lover. Join me as I share beauty news and cosmetic and accessories reviews.


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News and Calendar - About the University, University of Gothenburg, Sweden
This is where you can find the latest news from the University of Gothenburg in English. In our calendar you will find the latest events open for an English speaking audience.
Body ideal determines men and women's use of doping agents
[27 Jan 2020] Fitness doping is still common despite well-known risks. Researchers at the University of Gothenburg and Linnaeus University have made an ethnographic study to understand the processes by which a person becomes or unbecomes a ¿fitness doper¿.
New species of antibiotic-resistant bacteria found in infected wound
[16 Jan 2020] A hitherto unknown antibiotic-resistant bacteria species, in the same family as E. coli and Salmonella spp., has been found and classified in Sweden. The proposed taxonomic name of the species, the first of the new genus, is Scandinavium goeteborgense, after the city of Gothenburg, where the bacterium was isolated and the research was done.
Human caused biodiversity decline started millions of years ago
[15 Jan 2020] The human-caused biodiversity decline started much earlier than researchers used to believe. According to a new study published in the scientific journal Ecology Letters the process was not started by our own species but by some of our ancestors.


American Legion, China Post #1, Expat Post-Great for those frequent overseas travelers.
Above is outstanding and well organized.
All links tested and working on 19 Nov 2007 in Washington DC. Please report bad links found on these pages.
If you have comments, improvements, or additional links to add, please email me! I look forward to hearing from you! Many new links are constantly added from readers sending them to me! We want this site as interactive and user-friendly as possible.
To navigate this site use the drop-down menu at top. Also look for sub sections listed on the left.
Storybasket.com A Korean & English site full of stories about cross culture success and funny stories.
We have a new feature on Webmaster or Mrs. Webmaster's various sites, a search engine for SecurityMgr.Info, S2online.org (Military Security Managers), Storybasket Asian Cross Culture, and American Legion CP1 .
This website was started in 1991 to assisting security managers and making soldiers target smart on foreign countries.
Date of last edit: 19 November 2007 19:20 time is Washington DC.


This unit will be the next generation of kiln controllers with its modern and intuitive user platform. But, because results are what counts, this one also includes the knowledge that is at the heart of every Bartlett controller. We design, manufacture and sell all of our controllers with our customers at the forefront of that process and we insist on procedures and systems to continue to be a reliable and consistent resource for artists. The control strategies that have produced so many successful firings with Bartlett controllers will only be enhanced by this new format of display and user interface.


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Satyr Mask
by Mark Cartwright
A Roman satyr mask in marble. 2nd century CE. (Capitoline Museums, Rome)
Mark Cartwright
Mark is a history writer based in Italy. His special interests include pottery, architecture, world mythology and discovering the ideas that all civilizations share in common. He holds an MA in Political Philosophy and is the Publishing Director at WHE.
Uploaded by Mark Cartwright, published on 17 January 2016 under the following license: Creative Commons Attribution-NonCommercial-ShareAlike. This license lets others remix, tweak, and build upon this content non-commercially, as long as they credit the author and license their new creations under the identical terms. When republishing on the web a hyperlink back to the original content source URL must be included. Please note that content linked from this page may have different licensing terms.
Images107
Ancient Greek Tragedy
Greek tragedy was a popular and influential form of drama performed...
Ancient Greek Theatre
Greek theatre began in the 6th century BCE in Athens with the performance...
Satyrs (aka silens) are figures from Greek mythology who were followers...
Greek Theatre Architecture
The ancient Greeks built open-air theatres where the public could...
Elizabethan Theatre
Elizabethan theatre, sometimes called English Renaissance theatre...
Cyclops (Play)
The satyr-play The Cyclops was written by Euripides, one of the...
Cartwright, M. (2016, January 17). Satyr Mask. World History Encyclopedia. Retrieved from https://www.worldhistory.org/image/4442/satyr-mask/
Cartwright, Mark. "Satyr Mask." World History Encyclopedia. Last modified January 17, 2016. https://www.worldhistory.org/image/4442/satyr-mask/.
Cartwright, Mark. "Satyr Mask." World History Encyclopedia. World History Encyclopedia, 17 Jan 2016. Web. 22 Jan 2022.
We are a non-profit organization.
Our mission is to engage people with cultural heritage and to improve history education worldwide. Please support World History Encyclopedia Foundation. Thank you!


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Barraquito () is a coffee liqueur commonly available on Tenerife (one of the Canary Islands), also known as zaperoco.

Etymology

Description
The barraquito is a multi-layered coffee liqueur drink (though non-liqueur versions are available) normally served in a glass to enable easy viewing of the different layers.

Ingredients
The layers of a barraquito are normally:
 Coffee
 Licor 43
 Frothed milk
 Condensed milk

Other ingredients typically used:
 Lemon peel
 Cinnamon

Preparation
The condensed milk is first added, followed by the liqueur, espresso and lemon peel (in this order).  Milk (can be frothed by any means available) is then added and cinnamon is sprinkled on top.

Regional variations
The barraquito is often known as a "zaperoco" in northern areas of Tenerife, it can be also spelled as "Saperoco". In some places and menues, Barraquito is served without alcohol, while Zaperoco/Saperoco is served with alcohol.

References

External links

Coffee liqueurs
Canary Islands cuisine

redpajama_set_name: RedPajamaWikipedia