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

With the successful commissioning of \mbox{\it JWST}, the detailed study of rest-frame optical emission of distant, high-redshift ($z>3$) galaxies has now opened up. Already, dozens of arcmin$^2$ of deep $>2$~\textmu m imaging have been obtained \citep[e.g.][]{Bagley22}. This has allowed us to identify samples of $z>10$ galaxies for the first time \citep[e.g.][]{Adams22,Atek22,Castellano22,Donnan22, Finkelstein22c, Naidu22a}, probe the rest-frame optical spectral energy distributions at $z>6$ \citep[e.g.][]{Adams22}, and study optical morphologies to high-redshift \citep[e.g.][]{Ferreira22a, Ferreira22b, Kartaltepe22}. At the same time, the first spectroscopic constraints have emerged making use of both \mbox{\it JWST}'s multi-object (MOS) and wide field slitless spectroscopic (WFSS) modes to study distant, high-redshift galaxies \citep[e.g.][]{Kashino22, Matthee23, Sun23, Tacchella22, Trump22, Trussler22, Curti23, Katz23}. With many more spectroscopic observations underway, large samples will soon emerge, providing new insights into the physical properties of distant galaxies as well as accurately constraining their redshifts.

The primary target of spectroscopic studies of distant galaxies is the various rest-frame optical emission lines. These not only permit an unambiguous determination of the redshift, but carry a wealth of information about the source of ionising photons and the composition and properties of the interstellar medium (ISM) in these distant galaxies.

While a range of optical lines are now potentially accessible, in this work we focus on the [\ion{O}{III}]$\lambda\lambda 4960,5008$\AA (hereafter [\ion{O}{III}]) doublet. In this work we consider both the combined line luminosity and EW denoted by [\ion{O}{III}]\ and individual lines denoted by e.g. [\ion{O}{III}]$\lambda 5008{\rm\AA}$. The combined [\ion{O}{III}]\ line flux is, at least for $Z\approx 0.001-0.01$, similar to H$\alpha$ while also being accessible at higher-redshift, $z\approx 9$ (c.f. $z\approx 6.6$ for H$\alpha$) with \mbox{\it JWST}'s near-infrared instruments alone. For typical metallicities this line is correlated with the ionising photon production, though is also sensitive to extreme metallicities ($Z<0.001$, $Z>0.01$) and the conditions of the ISM. Crucially, observational constraints have already emerged for statistically useful samples of galaxies \citep[e.g.][]{Sun23, Matthee23}.

To fully realise the constraining potential of these observations, in this work we make predictions for the [\ion{O}{III}]\ properties of galaxies at $z=5-10$ using the First Light And Reionisation Epoch Simulations \citep[\mbox{\sc Flares}][]{FLARES-I}. \mbox{\sc Flares}\ is a suite of hydrodynamical simulations employing the \mbox{\sc{Eagle}}\ physics model \citep{schaye_eagle_2015, crain_eagle_2015}, but with a strategy designed to efficiently extend the range of masses and luminosities simulated relative to the original \mbox{\sc{Eagle}}\ reference simulation. \mbox{\sc Flares}\ has also been used to study the evolution of galaxy sizes \citep{FLARES-IV, FLARES-IX}, colours \citep{FLARES-VI}, star formation and metal enrichment histories \citep{FLARES-VII}, and the emergence of passive galaxies \citep{FLARES-VIII}. This work builds on earlier efforts to model the nebular line emission in large samples of simulated high-redshift galaxies \citep[e.g][]{Wilkins2013d, Wilkins20, FLARES-II}. In this work we explore predictions for a range of properties including the [\ion{O}{III}]\ luminosity function, the correlation of $L_{[\ion{O}{III}]}$ with the UV luminosity, the equivalent width distribution, the correlation with physical properties, and the impact of dust attenuation.  We also compare these predictions with recent observational constraints.

This paper is structured as follows: in Section \ref{sec:theory} we explore the key physics driving [\ion{O}{III}]\ emission in star forming galaxies, including the dependence on the star formation and metal enrichment history (\S\ref{sec:theory:sfzh}), geometry (\S\ref{sec:theory:geometry}), dust (\S\ref{sec:theory:dust}), and the assumed initial mass function and stellar population synthesis model (\S\ref{sec:theory:spsimf}). In Section \ref{sec:flares} we describe the \mbox{\sc Flares}\ project, including details of our spectral energy distribution modelling procedure (\S\ref{sec:flares:sed}). Then in Section \ref{sec:predictions} we present our predictions for the [\ion{O}{III}]\ properties of galaxies in \mbox{\sc Flares}. In this section we also explore the impact of dust  (\S\ref{sec:predictions:dust}) and the correlation of [\ion{O}{III}]\ emission with key physical properties  (\S\ref{sec:predictions:physical}). In Section \ref{sec:observations} we then compare our predictions with recent observations from \mbox{\it Hubble}\ and \mbox{\it JWST}. We then summarise our findings in this work and present our conclusion in Section \S\ref{sec:conc}.

While this article is focused on the prominent [\ion{O}{III}]\ doublet we also make predictions for several other strong rest-frame optical emission lines including [\ion{O}{II}] 372.6,372.9 nm, [\ion{Ne}{III}]386.9,396.7 nm, \mbox{H$\beta$}, and \mbox{H$\alpha$}. These are presented in the Appendix.

\section{Conclusions}\label{sec:conc}

In this work we have explored the [\ion{O}{III}]\ properties of the galaxy population in the First Light And Reionisation Epoch Simulations (\mbox{\sc Flares}). The \mbox{\sc Flares}\ strategy enables us to predict the properties of galaxies over a wide range of masses and luminosities at high-redshift.

Our main conclusions are:

\begin{itemize}
    \item The [\ion{O}{III}]\ luminosity function (LF) predicted by \mbox{\sc Flares}\ declines sharply with redshift with the density of sources dropping by $\approx 1$ dex from $z=5$ to $10$.  The bright-end of the LF is strongly impacted by dust with a suppression of 1 dex at $L\sim 10^{43.5}\ {\rm erg/s}$. While the faint end of the LF is well matched to recent spectroscopic constraints \citep[][]{Sun23, Matthee23} we predict fewer very bright sources than \citet{Matthee23} with one possible explanation being comsic variance.

    \item We predict a flat, un-evolving, relationship between the far-UV and [\ion{O}{III}]\ line luminosities. While the intrinsic ratio falls to higher luminosity due to the effect of increasing metallicity this is moderated by the growing impact of dust.

    \item We predict a median [\ion{O}{III}]\ rest-frame equivalent width (EW) of $\approx 500$\AA\ at $z=5$. This declines slightly with far-UV luminosity and stellar mass and increases to higher-redshift. At low UV luminosities dust-attenuated EWs are slightly smaller than the intrinsic values. However, at higher luminosities ($M<-21$), dust-attenuated EWs are slightly higher than the intrinsic values indicating that the continuum emission is more heavily attenuated than the line. The interpretation here is that the young [\ion{O}{III}]\ producing stellar population are preferentially found on the outskirts of galaxies compared to the continuum producing population. We find that the [\ion{O}{III}]\ EW correlates weakly with specific star formation rate but more strongly with ionising photon production efficiency. The relationship with metallicity is more complex with two clear branches.

    \item Our median EWs are consistent with both recent photometric \citep[][]{deBarros19_OIIIHbeta, Endsley22} and spectroscopic \citep{Sun23, Matthee23} constraints. However, we fail to predict the tail of galaxies with extremely high ($>2000$\AA) EWs found by these studies possibly suggesting an additional source of ionising photons in these systems.

    \item We predict [\ion{O}{III}] 5008\AA/H$\beta$ ratios of $\approx 4-5$, slightly smaller than those found by \citet{Matthee23}. However, our ratios are strongly affected by our assumed reference ionisation parameter.

\end{itemize}

Spectroscopic constraints of galaxies in the distant Universe will imminently be transformed by surveys such as JADES and CEERS. Together with other cycle 1/2 observations these will vastly increase the sample size and dynamic range of spectroscopic observations of [\ion{O}{III}]\ and other lines yielding new constraints on physical models in this epoch of the Universe's history.

\section{Comparison with Observational Constraints}\label{sec:observations}

We now turn our attention to a comparison with recent observational constraints from \mbox{\it Hubble}, \mbox{\it Spitzer}, and \mbox{\it JWST}, including \citet{deBarros19_OIIIHbeta},  \citet{Endsley22}, \citet{Matthee23}, and \citet{Sun23}. The former two studies infer the [\ion{O}{III}]\ + \mbox{H$\beta$}\ properties from broadband photometry, while the latter two use spectroscopic observations recently obtained by \mbox{\it JWST}.

\subsection{Photometric Constraints}

The predicted strength of the combination of the [\ion{O}{III}]\ and \mbox{H$\beta$}\ emission is sufficient to significantly boost broadband fluxes by up-to $\approx 0.3$ dex \citep[e.g.][]{Wilkins2013d, Wilkins20}. With one band encompassing the line emission and a second probing the (strong line emission free) continuum, it is then possible to infer the luminosities and equivalent widths of these combined lines. In particular, combining \mbox{\it Hubble}\ and \mbox{\it Spitzer}/IRAC observations \citep[e.g.][]{Smit2014, Roberts_Borsani_2016, deBarros19_OIIIHbeta, Endsley2021} or, more recently, \mbox{\it JWST}\  \citep[e.g.][]{Endsley22}, it is possible to constrain the combined [\ion{O}{III}]\ and \mbox{H$\beta$}\ emission.

In Figure \ref{fig:observations} we compare the combined [\ion{O}{III}]\ + \mbox{H$\beta$}\ EWs predicted by \mbox{\sc Flares}\ with photometric constraints from \citet{deBarros19_OIIIHbeta} and \citet{Endsley22} at $z=6-9$. In both cases we find good agreement between the predicted and observed median EWs. This supports the findings of \citet{FLARES-VI} where we made a direct comparison between the broadband \mbox{\it Hubble}\ and \mbox{\it Spitzer}\ colours of observed galaxies and galaxies predicted by \mbox{\sc Flares}, finding good agreement. However, while we broadly reproduce the median EW, we fail to reproduce the high-EW tail observed in both \citet{deBarros19_OIIIHbeta} and \citet{Endsley22}. In the context of [\ion{O}{III}]\ driven by stellar populations there is little remaining model flexibility, since our assumptions tend to maximise the possible EWs. For example, assuming an alternative reference ionisation parameter $U$ would not significantly increase EWs since our adopted value ($0.01$) maximises the EW, as demonstrated in Figure \ref{fig:theory_U} (\S\ref{sec:theory:geometry}). This suggests the explanation lies either with the observations themselves, or there is a significant additional source of ionising photons present in high-redshift galaxies. While \mbox{\sc Flares}\ predicts AGN are present in these galaxies, their contribution to the LyC luminosity is, on average, relatively small (see Kuusisto et al., \emph{in-prep}).

\begin{figure}
    \includegraphics[width=\columnwidth]{figs/EW_observations_6.pdf}
    \includegraphics[width=\columnwidth]{figs/EW_observations_7.pdf}
    \includegraphics[width=\columnwidth]{figs/EW_observations_8.pdf}
	\caption{Comparison between our predicted [\ion{O}{III}]\ + \mbox{H$\beta$}\ equivalent widths and observations from \citet{deBarros19_OIIIHbeta}, \citet{Endsley22}, and \citet{Matthee23} at $z=5-9$. \label{fig:observations}}
\end{figure}

\subsection{Spectroscopic constraints}\label{sec:observations.spectroscopic}

As noted in the introduction, a handful of spectroscopic constraints on [\ion{O}{III}]\ are now available at $z>6$. At present these samples are small, but will rapidly grow thanks to large spectroscopic programmes such as JADES and CEERS.

\citet{Sun23} presented observations of four serendipitously discovered emission line galaxies at  $z = 6.11 - 6.35$ in \mbox{\it JWST}\ NIRCam wide field slitless spectroscopy (WFSS)  comissioning data. These galaxies exhibit [\ion{O}{III}] 5008\AA\ EWs ranging from $100-1200{\rm\AA}$ with a median [\ion{O}{III}]\ + \mbox{H$\beta$}\ EW $546\pm 77$\AA, consistent with our predictions of $\approx 500-600{\rm\AA}$ at the same redshift and luminosity range. \citet{Sun23} also present constraints on the [\ion{O}{III}] 5008\AA\ luminosity function, and these are presented in Figure \ref{fig:LF}. These are somewhat higher than the predictions from \mbox{\sc Flares}, but the sample size is small and consequently the statistical uncertainties are very large. Since the observations are based on a single NIRCam pointing there is also the possibility of significant field-to-field variation (see Thomas \emph{et al.} - in-prep).

More recently, \citet{Matthee23} presented spectroscopic constraints from the \mbox{\it JWST}\ NIRCam WFSS Emission-line galaxies and Intergalactic Gas in the Epoch of Reionization \citep[EIGER,][]{Kashino22} survey. \citet{Matthee23} present both pure spectroscopic constraints alongside spectro-photometric constraints, combining line fluxes from the WFSS with photometry from the NIRCam imaging.

The combined [\ion{O}{III}]\ + \mbox{H$\beta$}\ equivalent widths of the \citet{Matthee23} observations are shown in Figure \ref{fig:observations}. Here we choose to compare with the spectro-photometric constraints since these allow a better estimation of the continuum flux than the pure spectroscopic observations alone. We find good agreement between the predicted and observed median of the EW distribution. However, like with the photometric constraints we find an excess in the number of high-EW sources.

\citet{Matthee23} also constrain the relationship between the far-UV and [\ion{O}{III}]\ luminosity, shown in Figure \ref{fig:L} and the [\ion{O}{III}] 5008\AA\ luminosity function, shown in Figure \ref{fig:LF}. The normalisation of the $L_{\rm FUV}$-$L_{[\ion{O}{III}]}$ relationship matches that predicted by \mbox{\sc Flares}, though the slope is somewhat steeper, resulting in fainter galaxies having higher ratios than predicted by \mbox{\sc Flares}. At faint ($L_{[\ion{O}{III}]}<10^{43}\ {\rm erg/s}$) luminosities the \mbox{\sc Flares}\ predictions provide an excellent match to EIGER luminosity function. However, at brighter luminosities the EIGER constraints tend to be higher than predicted by \mbox{\sc Flares}, suggesting an excess of bright [\ion{O}{III}]\ emitting galaxies. One possible explanation here is cosmic variance. Indeed, the EIGER field contains an over-density at $z\approx 6.77$ to which three of four sources with $M_{\rm FUV}<-22$ belong. While the EIGER constraints lie above our predictions, which include dust attenuation, they are however comparable to our intrinsic predictions. Another possibility is then that we have over-predicted the amount of dust attenuation in these systems.

Spectroscopic observations also have the advantage that they can separate the contributions of [\ion{O}{III}]\ and \mbox{H$\beta$}, allowing us to measure line ratios.  {\citet{Matthee23} measure [\ion{O}{III}] 5008/\mbox{H$\beta$}\ (R3) line ration in their sample, finding an average value of $6.3$. This is slightly larger than our predicted typical values ($4-5$) possibly suggesting the need for higher ionisation parameters (see \S\ref{sec:theory:geometry}).

\section{Theoretical Background}\label{sec:theory}

Ionising photons produced by massive stars, active galactic nuclei (AGN), or other phenomena (e.g. shocks) lead to the formation of \ion{H}{II} regions. Within these regions various physical processes result in the formation of nebular line and continuum emission. The strength of individual emission lines are sensitive to the shape and normalisation of the ionising spectrum, alongside the properties of the ionised region, including its geometry, composition, and other physical properties.

Amongst the most prominent and useful lines is the [\ion{O}{III}]\ doublet. In this section we explore how the luminosities and equivalent widths of the [\ion{O}{III}] doublet are affected by the star formation history, metallicity, and geometry. To do this we employ smooth parametric star formation histories, a single metallicity shared by both the stellar population and surrounding gas, and a simple screen model for reprocessing by dust and gas (i.e. stellar populations are all equally affected by dust). Initially, we assume the following fiducial parameters and model choices: to model the stellar emission we use the v2.2.1 of the Binary Population And Spectral Synthesis (BPASS) stellar population synthesis (SPS) model and  a \citet{chabrier_galactic_2003} initial mass function (IMF), while to model the nebular emission we use version 17.03 of the \texttt{cloudy} photo-ionisation code \citep{Ferland2017} and assume a reference ionising parameter ($U_{\rm ref}$) of $0.01$, a solar abundance pattern, and no escape of ionising photons. Most of these assumptions are explored in this section.

\subsection{Star formation and metal enrichment history}\label{sec:theory:sfzh}

In a stellar population the production of Lyman-continuum (LyC) photons is dominated by hot, massive, and short lived stars. Consequently, the LyC luminosity ($\dot{n}_{\rm LyC}$) drops precipitously as the stellar population ages. This is demonstrated in Figure \ref{fig:theory_log10Q}, where we show the specific LyC luminosity as a function of age and metallicity. This reveals that the LyC luminosity drops by a factor of $\approx 10^{4}$ as a population ages from $t=1\to 100\, {\rm Myr}$. As lower-metallicity stars can attain higher temperatures, the LyC luminosity is lower at high metallicity, at least at young ages ($<10\ {\rm Myr}$). For older stellar populations this trend reverses as the most massive stars evolve off the main sequence faster.

\begin{figure}
	\includegraphics[width=\columnwidth]{figs/theory_log10Q.pdf}
	\caption{The specific ionising photon luminosity of a simple stellar population as a function of age and metallicity assuming BPASS v2.2.1 and \citet{chabrier_galactic_2003} IMF with $m_{\rm up}=300\ {\rm M_{\odot}}$.\label{fig:theory_log10Q}}
\end{figure}

The consequence of this strong dependency on age and metallicity is that any emission line is strongly sensitive to the star formation and metal enrichment history. In Figure \ref{fig:theory_sfh} we explore how the \emph{specific} (i.e. per unit stellar mass formed) [\ion{O}{III}]\ luminosity, equivalent width (EW), and ratio to the \mbox{H$\beta$}\ luminosity are affected by the star formation history. Here we present results assuming four simple star formation histories: an instantaneous burst, an exponentially declining ($\tau=-100$ Myr), constant, and exponentially increasing star formation ($\tau=100$ Myr). Unsurprisingly in each case the specific luminosity and EW drops, at least initially. With no replenishment of massive stars in the instantaneous model the luminosity and EW drop by four orders of magnitude over $t=1\to 100\, {\rm Myr}$. For the other models both drop more slowly, with the luminosity (EW) dropping by $\approx 10\times$ ($\approx 4\times$) over $t=1\to 100\, {\rm Myr}$. At this point the exponentially increasing model plateaus as the rapidly increasing star formation rate balances the accumulation of longer lived lower mass stars. Conversely in the exponentially declining model the luminosity and EW rapidly drop, eventually joining an instantaneous burst. In the constant model the specific luminosity and EW drop at a near constant fractional rate. For scenarios with continuing star formation the [\ion{O}{III}]/\mbox{H$\beta$}\ luminosity ratio is largely constant since the shape of the ionising spectrum remains roughly constant. Conversely, for an instantaneous burst the [\ion{O}{III}]/\mbox{H$\beta$}\ ratio drops as the population ages due to the changing shape of the ionising spectrum.

\begin{figure}
	\includegraphics[width=\columnwidth]{figs/theory_sfh.pdf}
	\caption{The specific [\ion{O}{III}]\ luminosity, [\ion{O}{III}]\ equivalent width, and of [\ion{O}{III}]/\mbox{H$\beta$}\ luminosity ratio as a function of the duration of star formation assuming four different star formation histories: an instantaneous burst (dotted line), exponentially decreasing star formation (dot-dashed line), constant star formation (solid line), and exponentially increasing star formation (dashed line), and three metallicities: $Z=10^{-4},\ 10^{-3}, 10^{-2}$. \label{fig:theory_sfh}}
\end{figure}

Figure \ref{fig:theory_sfh} also presents predictions for each star formation history scenario for three different metallicities: $Z=10^{-4},\ 10^{-3},$ and $10^{-2}$. Metallicity has an impact through both changing the ionising continuum normalisation and shape, and changing the composition of the nebular region itself. To show this more clearly, in Figure \ref{fig:theory_Z} we show the luminosity, EW, and [\ion{O}{III}]/\mbox{H$\beta$}\ ratio as a function of metallicity assuming 10 Myr constant star formation. In the top (luminosity) panel we also show the LyC luminosity. While the LyC luminosity increases to lower metallicity, the [\ion{O}{III}]\ luminosity (and thus EW) reaches a peak at $Z\sim 0.005$, dropping rapidly on either side. At low-metallicity the decrease is driven by dropping abundance of Oxygen, while the drop to high-metallicities is due to both the falling LyC luminosity and changing shape of the ionising spectrum.

\begin{figure}
	\includegraphics[width=\columnwidth]{figs/theory_Z.pdf}
	\caption{The specific [\ion{O}{III}]\ luminosity, [\ion{O}{III}]\ equivalent width, and of [\ion{O}{III}]/\mbox{H$\beta$}\ luminosity ratio as a function of metallicity assuming 10 Myr constant star formation. Also shown on the top panel is the sensitivity of the LyC luminosity.\label{fig:theory_Z}}
\end{figure}

\subsubsection{Composition}\label{sec:theory:composition}

In our modelling so far we have assumed that the composition of the nebular gas follows a Solar composition. However, at high-redshift, galaxies will be increasingly enhanced with $\alpha$-elements due to the shorter timescale for their production \citep{Steidel2016}. To explore the impact of $\alpha$-enhancement in Figure \ref{fig:theory_alpha} we show the specific [\ion{O}{III}]\ luminosity, [\ion{O}{III}]\ equivalent width, and [\ion{O}{III}]/\mbox{H$\beta$}\ luminosity ratio as a function of metallicity for different $\alpha$-enhancements assuming 10 Myr constant star formation. Since the underlying stellar models assume Solar composition, this modelling is not self-consistent; nevertheless, it allows us to explore the potential impact. This reveals that boosting the enhancement to [$\alpha$/Fe]$=0.6$ boosts [\ion{O}{III}]\ luminosities and EWs by $\approx 0.1$ dex at $Z<0.003$. At $Z> 0.005$ the effect becomes small and leads to a suppression at super-solar metallicities.

\begin{figure}
	\includegraphics[width=\columnwidth]{figs/theory_alpha.pdf}
	\caption{The same as Figure \ref{fig:theory_Z} but showing different levels of $\alpha$-enhancement in the nebular gas. \label{fig:theory_alpha}}
\end{figure}

\subsubsection{Geometry}\label{sec:theory:geometry}

In our \texttt{cloudy} modelling the geometry of the H\textsc{ii} region is encapsulated by the LyC escape fraction and the ionisation parameter ($U$). $U$ encodes the the number of LyC photons per atom.

In the modelling thus far we have assumed a fixed reference ionisation parameter of $U_{\rm ref}=0.01$ referenced at $t=1$ Myr and $Z=0.01$. What this means is that the actual ionisation parameter assumed by our \texttt{cloudy} implementation varies according to the metallicity and age of the stellar population such that,
\begin{equation}
    U = U_{\rm ref}\left(\frac{Q}{Q_{\rm ref}}\right)^{1/3}
\end{equation}
where $U$ and $Q$ are the ionisation parameter and ionising photon luminosity of the stellar population and $U_{\rm ref}$ and $Q_{\rm ref}$ are that for the reference population.

To see how the ionisation parameter affects our predictions, in Figure \ref{fig:theory_U} we show the specific luminosity, EW, and [\ion{O}{III}]/\mbox{H$\beta$}\ line ratio as a function of metallicity but assuming several different reference ionisation parameters, $\log_{10}U_{\rm ref} = -4\to 0$. This reveals the complex sensitivity of [\ion{O}{III}]\ to $U$. The [\ion{O}{III}]\ mass-weighted luminosity peaks assuming $\log_{10}U_{\rm ref} \approx -2$ (i.e. our default value) at $Z=0.003$. The location of the peak is sensitive to the choice of $U$ shifting to lower metallicity with higher $U$. This shift is sufficient such that at very low metallicity ($Z<0.0001$) the [\ion{O}{III}]\ emission is highest for higher values of $U$.

\begin{figure}
	\includegraphics[width=\columnwidth]{figs/theory_U.pdf}
	\caption{As Figure \ref{fig:theory_Z} but showing the impact of varying the reference ionisation parameter $U_{\rm ref}$.\label{fig:theory_U}}
\end{figure}

\subsubsection{Dust}\label{sec:theory:dust}

Like any other optical photons, the [\ion{O}{III}]\ line emission is susceptible to dust attenuation. For a simple screen dust geometry, EWs will be unaffected by dust since both the continuum and line emission would be attenuated by the same amount. In reality, however, dust and stars have a more complex geometry, likely leaving EWs sensitive to dust attenuation. For example, a model in which young stars and their associated \ion{H}{II} regions are attenuated more strongly than older stars would naturally result in line emission suffering higher attenuation than the underlying continuum, reducing the equivalent width. On the other hand, if star formation is preferentially taking place on the outskirts of galaxies,  where the attenuation is lower, then the attenuation of the overall continuum could be higher, boosting EWs relative to their intrinsic values. This is an important consideration, since \mbox{\sc Flares}\ includes both a birth cloud component and a wider attenuation for each star particle determined by the distribution of metals along the line-of-sight. In the context of the \mbox{\sc Flares}\ predictions this is explored in \ref{sec:predictions:dust}.

\subsection{Initial Mass Function and Stellar Population Synthesis Model}\label{sec:theory:spsimf}

Finally, any predicted observational quantity is also going to be affected by the choice of Initial Mass Function (IMF) and Stellar Population Synthesis (SPS) model. In Figure \ref{fig:theory_sps} we show the predicted luminosity and EW as a function of metallicity for three different SPS models, including BPASS (our default),  the Flexible Stellar Population Synthesis \citep[FSPS][]{FSPSI} code, and the \citet{BC03} (BC03) models. Due the inclusion of binary interactions the BPASS model generally yields higher LyC luminosities, resulting in higher line luminosities and EWs \citep{Stanway2016}. At $Z<0.001$ FSPS yields slightly higher luminosities, but EWs that are $\approx 50\%$ higher than BPASS due to fainter continuum emission.

\begin{figure}
	\includegraphics[width=\columnwidth]{figs/theory_sps.pdf}
	\caption{As Figure \ref{fig:theory_Z} but for two additional population synthesis models: FSPS and BC03. \label{fig:theory_sps}}
\end{figure}

Since the IMF controls the relative proportions of stars and line emission is driven by the most massive stars the luminosity, and potentially EWs, will be sensitive to the shape of the IMF. In Figure \ref{fig:theory_imf} we show the predicted specific line luminosities and EWs as a function of the high-mass slope of the IMF ($\alpha_{3}$) using the BPASS and FSPS models which include this flexibility. In both FSPS and BPASS the parameter $\alpha_{3}$ describes the slope of the IMF at $>1\ {\rm M_{\odot}}$ (c.f. Salpeter: $\alpha=2.3$). We do this for three metallicities but in each case assume 10 Myr constant star formation. Unsurprisingly, this reveals that line luminosities are strongly impacted by the choice of $\alpha_{3}$ with the line luminosity increasing by $\approx 0.5$ dex for changes to the slope of 0.35. However, EWs are only subtly affected since the optical continuum emission is also enhanced.

\begin{figure}
	\includegraphics[width=\columnwidth]{figs/theory_imf.pdf}
	\caption{The dependence of the line luminosity and EW on the high-mass slope of the IMF $\alpha_{3}$ assuming BPASS and FSPS.\label{fig:theory_imf}}
\end{figure}

\section{First Light And Reionisation Epoch Simulations}\label{sec:flares}

In this study we make use of the First Light And Reionisation Epoch Simulations (\mbox{\sc Flares}). \mbox{\sc Flares}\ is introduced in \citet{FLARES-I} and \citet{FLARES-II} and we refer the reader to those papers and references therein for a detailed introduction. In brief, \mbox{\sc Flares}\ is a suite of hydrodynamical re-simulations. The core\footnote{In addition to the core runs \mbox{\sc Flares}\ includes a range of simulations exploring changes to the physics model.} \mbox{\sc Flares}\ suite adopts the AGNdT9 variant of the \mbox{\sc{Eagle}}\ simulation project \cite[][]{schaye2015_eagle,crain2015_eagle} with identical resolution to the \mbox{\sc{Eagle}}\ reference run. The core suite consists of 40 $14/h\ {\rm cMpc}$ radius re-simulations of regions selected from a large $(3.2\ {\rm Gpc})^3$ dark matter only simulation. The selected regions span a large range in over-density (at $z\approx 4.7$): $\delta + 1 \approx -1\to 1$, with over-representation of the extremes of the density distribution. This yields a large range of galaxy and halo masses across a wide range of environments. This \mbox{\sc Flares}\ strategy allows us, by appropriately weighting each galaxy, to predict galaxy distribution functions and scaling relations across a wider range of masses and luminosities than possible in a similarly sized periodic volume.

\subsection{Spectral Energy Distribution modelling}\label{sec:flares:sed}

The spectral energy distribution (SED) modelling of galaxies in \mbox{\sc Flares}\ is described in depth in \citet{FLARES-II}. In short, we associate every star particle\footnote{The initial star particle mass is $\approx 2\times 10^{6}\ {\rm M_{\odot}}$.} in the simulation with a pure stellar SED based on its mass, age, and metallicity using v2.2.1 of the Binary Population And Spectral Synthesis \cite[BPASS]{BPASS2.2.1} stellar population synthesis (SPS) library, and assume a \cite[]{chabrier_galactic_2003} initial mass function (IMF).

In the top panel of Figure \ref{fig:flares} we present the \emph{specific} (i.e. per unit stellar mass) LyC photon production rate predicted for galaxies in \mbox{\sc Flares}. This quantity simply depends on the star formation and metal enrichment histories of galaxies, since it is independent of reprocessing by dust and gas. This reveals a clear downward trend at high-masses ($M_{\star}>10^{9.5}\ {\rm M_{\odot}}$) but remains flatter at lower mass. This is primarily due to the strong evolution of stellar metallicities across this mass-range \citep[see][]{FLARES-VII} combined with the strong dependence of LyC photon production on metallicity (see \S\ref{sec:theory:sfzh}). Figure \ref{fig:flares} also reveals significant redshift evolution, with the specific production rate declining by $\approx 0.6$ dex from $z=10\to 5$. Since the mass-metallicity relationship evolves weakly with redshift over this range, this decrease reflects the changing star formation histories of galaxies, in particular the increase in average ages.

\begin{figure*}
    \includegraphics[width=2\columnwidth]{figs/Q.png}
    \includegraphics[width=2\columnwidth]{figs/U.png}
	\caption{The evolution of the specific LyC photon production rate ($\dot{N}_{\rm LyC}/{\rm s^{-1}\ M_{\odot}^{-1}}$) [top] and effective ionisation parameter $U_{\rm eff}$ [bottom] from $z=5\to 10$ predicted by \mbox{\sc Flares}. The effective ionisation parameter in this context is the combination of all star particles weighted by their LyC luminosity. The thick grey line denotes the $z=5$ relation in both figures. \label{fig:flares}}
\end{figure*}

\subsubsection{Nebular emission modelling}

Once we have assigned a stellar SED we then associate each star particle with an ionisation bounded \ion{H}{II} region using version 17.03 of the \textsc{cloudy} photo-ionisation code \citep{Ferland2017}. Specifically, we use the pure stellar spectrum as the incident radiation field, assume the metallicity of the nebula is identical to the star particle, a solar abundance pattern, a covering fraction of 1 (corresponding to a LyC escape fraction of $\approx 0$ for an ionisation bound nebula) and a metallicity and age dependent ionisation parameter referenced at $t=1$ Myr and $Z=0.01$ of $U=0.01$. At other ages and metallicities the assumed ionisation parameter is scaled from this reference value using the ratio of the ionising luminosities of the two populations. A consequence of this is that nebular SEDs are formed from a wide range of ionisation parameters, with the maximum approximately that of the reference value. The bottom panel of Figure \ref{fig:flares} shows the effective (ionising photon luminosity weighted) ionisation parameter of galaxies in \mbox{\sc Flares}. Unsurprisingly, these are clustered around our reference ionisation parameter, though show some modest decrease to higher masses, reflecting the shift to higher metallicities. The assumption of a solar abundance pattern was a decision made to align with the BPASS SPS library. However, galaxies at high-redshift are observed \citep[e.g][]{Cullen21} and predicted \citep[e.g][]{FLARES-VII} to be strongly enhanced with $\alpha$-elements, including Oxygen. \citet{FLARES-VII} found typical enhancements of [$\alpha$/Fe]$=0.6-0.8$ at $5<z<10$. Our modelling in \S\ref{sec:theory:composition} revealed that this level of $\alpha$-enhancement can boost the [\ion{O}{III}]\ luminosity and EW fluxes by $\approx 0.1$ dex. In a future iteration of \mbox{\sc Flares}\ we plan to address this self-consistently by using the newest version (v2.3) of the BPASS models which include $\alpha$-enhancement in the stellar atmosphere modelling.

\subsubsection{Dust attenuation}

As described in \citet{FLARES-II} in \mbox{\sc Flares}\ we implement a two component dust attenuation model. First, we associate young stellar populations (with age less than 10 Myr, following \citet{CF00} that birth clouds disperse along these timescales) with a metallicity dependent dusty birth cloud. Secondly, for each star particle (and associated \ion{H}{II} region) we apply attenuation due to dust in the intervening inter-stellar medium. This is determined by calculating the line-of-sight surface density of metals along the spatial $z$-axis, for each star particle, and converting this to an optical depth. For both components we assume a simple $\lambda^{-1}$ dependence of the attenuation. In Vijayan et al. \emph{in-prep} we explore some of the wider features of this dust model.

\section{Predictions}\label{sec:predictions}

We now explore predictions for the [\ion{O}{III}]\ properties of galaxies in \mbox{\sc Flares}, including the [\ion{O}{III}]\ luminosity function, correlation with UV luminosity, and equivalent width distribution. We then explore how our predictions are impacted by dust attenuation and how the [\ion{O}{III}]\ EW correlates with other physical properties.

\subsection{[\ion{O}{III}]\ luminosity function}

We begin by exploring the shape and redshift evolution of the [\ion{O}{III}]\ luminosity function (LF), shown in Figure \ref{fig:LF}. The shape of the [\ion{O}{III}]\ LF broadly follows that of UV LF showing a clear drop at high-luminosities, consistent with an exponential like drop-off, and at fainter luminosities a power-law behaviour \citep{FLARES-II}. The UV LF itself tracks the evolution of galaxy stellar mass function \citep[GSMF, see ][]{FLARES-II} but with a steeper drop-off due to the effect of dust attenuation. Figure \ref{fig:LF} also shows the intrinsic [\ion{O}{III}]\ luminosity function revealing that, like the far-UV luminosity function \citep[see][]{FLARES-II}, the density of the brightest galaxies is suppressed by dust attenuation. The impact of dust attenuation is explored in more detail below in \S\ref{sec:predictions:dust}. Figure \ref{fig:LF} also includes a comparison with observations, this is discussed below in Section \ref{sec:observations}.

\begin{figure*}
    \includegraphics[width=2\columnwidth]{figs/LF_OIII5007.pdf}
	\caption{The evolution of the [\ion{O}{III}] 500.8nm luminosity function from $z=5\to 10$ predicted by \mbox{\sc Flares}. The dark thin line shows the \emph{observed} (dust-attenuated) luminosity function while the thicker fainter line shows the \emph{intrinsic} LF. The dashed line is the $z=5$ LF to highlight the evolution of the luminosity function. Observational constraints on the LF from \citet{Sun23} and \citet{Matthee23} are also shown at $z\approx 6$. \label{fig:LF}}
\end{figure*}

\subsection{[\ion{O}{III}]--UV luminosity relation}

The evolution of the [\ion{O}{III}]\ luminosity function across this redshift interval largely tracks that of the rest-frame far-UV luminosity function. To show this more clearly, in Figure \ref{fig:L} we show the relationship between the [\ion{O}{III}]\ luminosity and the far-UV luminosity, again from $z=5\to 10$. Firstly, this reveals a flat relationship, i.e. $L_{[\ion{O}{III}]}$ tracks $L_{\rm FUV}$. Since the most luminous galaxies in \mbox{\sc Flares}\ have significantly higher metallicity \citep[see][]{FLARES-VII} and that [\ion{O}{III}]\ luminosities drop precipitously with metallicity (see Figure \ref{fig:theory_Z}, \S\ref{sec:theory:sfzh}) this is perhaps surprising and we might naively expect to see a drop in $L_{[\ion{O}{III}]}/L_{\rm FUV}$ with $L_{\rm FUV}$. However, in \mbox{\sc Flares}\ [\ion{O}{III}]\ emission if generally less susceptible to dust than the UV compensating for the metallicity driven drop in [\ion{O}{III}]\ emission.

\begin{figure*}
    \includegraphics[width=2\columnwidth]{figs/LOIII-LFUV.pdf}
	\caption{The relationship between the [\ion{O}{III}]\ luminosity and the far-UV luminosity, expressed as a ratio, predicted by \mbox{\sc Flares}. The outlined black line show the median [\ion{O}{III}]\ luminosity while the grey line shows the median at $z=5$. The two shaded regions show the central 68\% and 95\% ranges. The dashed line shows the relationship obtained by \citet{Matthee23}. Note: the FUV luminosity included in the line ratio is expressed in units of erg/s not erg/s/Hz. \label{fig:L}}
\end{figure*}

\subsection{[\ion{O}{III}]\ equivalent width distribution}

Next, in Figure \ref{fig:EW}, we show predictions for the evolution of the relationship between the rest-frame [\ion{O}{III}]\ equivalent width and far-UV luminosity. This reveals a predominantly flat relationship at all redshifts, with a slight decline at the brightest luminosities. This decline is driven by the higher metallicity combined with slightly older ages in these galaxies \citep[see][]{FLARES-VII}.

\begin{figure*}
    \includegraphics[width=2\columnwidth]{figs/EW.pdf}
	\caption{The same as Figure \ref{fig:L} but showing the rest-frame equivalent width of [\ion{O}{III}]. \label{fig:EW}}
\end{figure*}

\subsection{[\ion{O}{III}]$\lambda 5008$-\mbox{H$\beta$}\ ratio}

An additional useful, observationally accessible, diagnostic is the ratio of the  [\ion{O}{III}]$\lambda 5008$ to \mbox{H$\beta$}\ line luminosities. Predictions from \mbox{\sc Flares}\ for this ratio are shown in Figure \ref{fig:lineratio}. Unlike the EW, this ratio is not particularly sensitive to the star formation history, at least for actively star forming galaxies. The ratio is however sensitive to extreme metallicities ($Z<0.001$, $Z>0.01$,) where it rapidly drops, as well as the ionisation parameter $U$. As the majority of \mbox{\sc Flares}\ galaxies span the range $Z=0.001-0.01$ and we assume a single reference ionisation parameter (and thus have a narrow range of effective ionisation parameters) it is not surprising that the \mbox{\sc Flares}\ predictions are tightly clustered around $\approx 5$.

\begin{figure*}
    \includegraphics[width=2\columnwidth]{figs/lineratio_log10FUV.pdf}
	\caption{The same as Figure \ref{fig:L} but showing the ratio of the [\ion{O}{III}]$\lambda 5008$ to H$\beta$ line luminosities. The point shows the observational constraints of \citet{Matthee23} for their full sample of 117 [\ion{O}{III}]\ emitters. \label{fig:lineratio}}
\end{figure*}

\subsection{Impact of reprocessing by dust}\label{sec:predictions:dust}

To further explore the impact of dust on our predictions, in Figure \ref{fig:reprocessing} we show the ratio of the intrinsic to attenuated line luminosities (top panel) and equivalent widths (bottom) as a function of the dust-attenuated far-UV luminosity.

As already hinted at in our comparison of the attenuated and intrinsic luminosity functions dust attenuation increases with both the far-UV and [\ion{O}{III}]\ luminosity. Compared to the intrinsic luminosity (not shown) the attenuation continues to increase with increasing luminosity. However, compared to the dust-attenuated (observed) luminosity the attenuation flattens since the most heavily obscured galaxies have lower observed luminosities. In the context of \mbox{\sc Flares}\ dust attenuation is due to both a birth cloud component, linked to the metallicity of each star particle, and an ISM component linked to the intervening surface density of metals. The more massive (and intrinsically bright) a galaxy generally the higher the stellar \citep[see][]{FLARES-VIII} and gas-phase metallicity. More massive galaxies also have larger gas reservoirs and thus metal (and dust) surface densities.

The effect of dust attenuation on equivalent widths is more complex. Our faintest galaxies show mild suppression peaking at $L_{\rm FUV}\approx 10^{29}\ {\rm erg/ s^{-1}/ Hz^{-1}}$ where the EW is reduced by 0.1 dex. At brighter far-UV luminosities the impact of dust on the EW dust declines and eventually leads to a small enhancement of EWs in the most UV luminous galaxies. The interpretation here is that in fainter galaxies, young [\ion{O}{III}]\ generating stellar populations undergo slightly higher dust attenuation than the wider continuum generating population. In the context of the \mbox{\sc Flares}\ model this is expected due to the addition of a birth cloud dust component. In the most luminous galaxies, which also roughly corresponds to the most attenuated systems, this additional birth cloud is sub-dominant to dust in the wider ISM. In these galaxies, the enhancement of EWs relative to the intrinsic values is   explained by the fact that the [\ion{O}{III}]\ producing stellar populations are preferentially found on the outskirts of galaxies compared to the continuum generating populations.

\begin{figure}
    \includegraphics[width=\columnwidth]{figs/reprocessing_ratio_OIIIHb.pdf}
    \includegraphics[width=\columnwidth]{figs/reprocessing_ratio_OIIIHbEW.pdf}
	\caption{The average (median) impact of dust attenuation of the [\ion{O}{III}]\ luminosity (top) and EW (bottom), both expressed as a function of the observed far-UV luminosity.  \label{fig:reprocessing}}
\end{figure}

\subsection{Correlation with Physical Properties}\label{sec:predictions:physical}

We next explore, in Figure \ref{fig:physical}, how the [\ion{O}{III}]\ equivalent width correlates with key physical properties, including the specific star formation rate, total stellar metallicity, the stellar metallicity of young stellar populations, and the ionising photon production efficiency $\xi_{\rm ion}$. Here, the star formation rate is defined as the mass of stars that have formed in the last 10 Myr, the stellar metallicity is the mass weighted stellar metallicity, and, in common with most observational studies, $\xi_{\rm ion}$ as the ratio of the Lyman continuum (ionising) photon production rate ($\dot{n}_{\rm LyC}$) to the rest-frame observed UV luminosity.

\begin{figure}
    \includegraphics[width=\columnwidth]{figs/physical.png}
	\caption{Comparison between the rest-frame [\ion{O}{III}]\ EW and the specific star formation rate, stellar metallicity (both total and young), and the ionising photon production efficiency $\xi_{\rm ion}$. The star formation rate is averaged over the preceding 10 Myr while the stellar metallicity is defined for all stellar populations. \label{fig:physical}}
\end{figure}

This reveals a correlation, albeit relatively weak ($r=0.44$), with specific star formation rate, such that galaxies with the highest [\ion{O}{III}]\ EW generally have higher specific star formation rates. This is expected since [\ion{O}{III}]\ emission is driven by young stars while the optical continuum includes a contribution from older stellar populations.

The relationship between the [\ion{O}{III}]\ EW and stellar metallicity is more complex, with two clear branches. Because of the steep shape of the galaxy stellar mass function, and the existence of a tight mass--metallicity relation, the vast majority of our galaxies have $Z_{\star}=0.001$. These faint, low-mass galaxies exhibit a range of EWs spanning $\approx 100-2000\ {\rm\AA}$ with the scatter driven by several effects, including the star formation history, dust, but crucially the metallicity of the [\ion{O}{III}]\ population, not just the overall metallicity. The second, upper, branch corresponds to more massive, luminous galaxies with higher-metallicities. The metallicities of the [\ion{O}{III}]\ producing stellar populations in these galaxies falls beyond the peak in the [\ion{O}{III}]\ luminosity--metallicity relation (see Figure \ref{fig:theory_Z}). Since this branch corresponds to the most massive and luminous systems it is also strongly impacted by dust attenuation, which has the effect of increasing the scatter in the EW but, as found previously, not significantly reducing it.

Finally, in the bottom panel of Figure \ref{fig:physical}, we show the relationship between the EW and the ionising photon production efficiency. This shows a clear correlation ($r=0.68$) such that the most extreme emitters have the largest production efficiencies. This is of course not a surprise considering [\ion{O}{III}]\ line emission is, at least in \mbox{\sc Flares}, driven by the production of ionising photons by massive stars.

\section*{Acknowledgements}

We thank the \mbox{\sc{Eagle}}\, team for their efforts in developing the \mbox{\sc{Eagle}}\, simulation code. We wish to thank Scott Kay and Adrian Jenkins for their invaluable help getting up and running with the \mbox{\sc{Eagle}}\, resimulation code.

This work used the DiRAC@Durham facility managed by the Institute for Computational Cosmology on behalf of the STFC DiRAC HPC Facility (www.dirac.ac.uk). The equipment was funded by BEIS capital funding via STFC capital grants ST/K00042X/1, ST/P002293/1, ST/R002371/1 and ST/S002502/1, Durham University and STFC operations grant ST/R000832/1. DiRAC is part of the National e-Infrastructure. We also wish to acknowledge the following open source software packages used in the analysis: \textsc{Scipy} \cite[][]{2020SciPy-NMeth}, \textsc{Astropy} \cite[][]{robitaille_astropy:_2013}, \textsc{Matplotlib} \cite[][]{Hunter:2007} and WebPlotDigitizer \cite[][]{Rohatgi2020}.

APV acknowledges support from the Carlsberg Foundation (grant no CF20-0534). PAT acknowledges support from the Science and Technology Facilities Council (grant number ST/P000525/1). DI acknowledges support by the European Research Council via ERC Consolidator Grant KETJU (no. 818930). CCL acknowledges support from a Dennis Sciama fellowship funded by the University of Portsmouth for the Institute of Cosmology and Gravitation. The Cosmic Dawn Center (DAWN) is funded by the Danish National Research Foundation under grant No. 140.

We list here the roles and contributions of the authors according to the Contributor Roles Taxonomy (CRediT)\footnote{\url{https://credit.niso.org/}}.
\textbf{Stephen M. Wilkins}: Conceptualization, Data curation, Methodology, Investigation, Formal Analysis, Visualization, Writing - original draft.
\textbf{Christopher C. Lovell,  Aswin P. Vijayan}: Data curation, Methodology, Writing - review \& editing.
\textbf{Nathan Adams, Joseph Caruana, Chris Concelice, James Donnellan, Dimitrios Irodotou, Jorryt Matthee, Pablo G. P\'erez-Gonz\'alez, William Roper, Louise Seeyave, Jack Turner}: Writing - review \& editing.

\section*{Data Availability}

The data associated with the paper will be made publicly available at \href{https://flaresimulations.github.io/data.html}{https://flaresimulations.github.io/data.html} on the acceptance of the manuscript.

\bibliographystyle{mnras}

redpajama_set_name: RedPajamaArXiv


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The Frugal Family Life: $1/1 Soft Scrub Coupon!
Here's a new $1/1 Soft Scrub Spray Product coupon this afternoon! I think these are priced around $3.00 or so which means after the double we will get a great deal!
I'm going to keep my eye out for a sale ad to price match to Nichols! Then use my double coupon on top to score the best deal! I'll let you know if I find a great match up!


I'd like to be into this show, but I'll admit that it's been a few days since I watched this episode and I can barely remember a thing about it, which doesn't recommend its enduring quality all that well. One element of the show that I didn't expect to be a big part was that of David Zayas' mobster, who survived a drive-by attempt at Charlie's home and now feels that he's indebted to the fake fortune teller. Charlie's diagnosis of his son's condition was a helpful way to make the link completely unbreakable, and it seemed silly that he brought Charlie along to tell him if his nephew had betrayed him and a simple nod from the guy meant that he should take him out by drowning him in the water used to make the donuts. Picking up a donut off the floor to eat it before commenting how good they are when they're hot was more than a bit much, and I'm not sure that this show needs scenery-chewing given its already over-the-top premise. The same goes for the character of Fonso in general, who makes a terrible and unconvincing villain, and his threat-making via home-cooked steak that Linda decided she just had to throw out. You'd think she would be slightly more discreet than to kiss her secret lover Gina in broad daylight outside their motel. I think this is enough of this show for me at this point, though I may revisit it at some point if it gets renewed for another season and seems like it could be worth it.


text:
https://blogs.wsj.com/indiarealtime/2016/01/15/mahindra-mahindras-new-kuv100-costs-6500-in-india/
India Real Time
Mahindra & Mahindra's New KUV100 Costs $6,500 in India
Santanu Choudhury
Jan 15, 2016 5:02 pm IST
The KUV100 launched in Maharashtra on Jan. 15, it is Mahindra & Mahindra's first compact sport-utility vehicle.
India's largest sport-utility vehicle maker Mahindra & Mahindra Ltd. is taking on the small-car market with a compact SUV it says offers the best of both worlds.
Launched on Friday, the KUV100 is powered by the smallest engine in Mahindra's portfolio. It is the first time the automaker has offered a gasoline-powered SUV.
Dealership prices start at 442,000 rupees ($6,568) for the 1.2-liter gasoline version, the top-end model costs around 591,000 rupees.
The 1.2-liter diesel engine model is pricier, starting at 522,000 rupees.
The KUV100 includes dual airbags, antilock brakes with electronic brake distribution, steering-mounted audio and phone controls, and remote keyless entry.
"I think we are creating a new class of car—a vehicle that combines the appeal of an SUV with the compactness of a hatchback," Anand Mahindra, chairman and managing director, of Mahindra & Mahindra, said in a recorded speech that was telecast at the launch.
Mahindra executives said they would target first-time, young customers who want to buy inexpensive, fuel-efficient hatchbacks.
They are also aiming to capitalize on the booming demand for SUVs in India, particularly compact versions and crossovers.
The company says the diesel model of the KUV100 can run up to 16 miles a liter, while the gasoline model has a mileage of 11 miles a liter.
Small cars such as Maruti's Swift, Hyundai's Grand i10 and Honda Motor Co.'s Jazz comprised 85.5% of the nearly 1.52 million cars sold in India in the first nine months of this fiscal year that ends March 31, according to the Society of Indian Automobile Manufacturers.
Industry experts say however that attracting potential small-car buyers could present an unprecedented challenge for Mahindra because there are so many of them available on the Indian market.
"Mahindra is the challenger in this segment and it isn't going to be easy as small-car buyers have a lot of trust in Maruti and Hyundai," said Anil Sharma, an analyst at IHS Automotive in India.
For breaking news, features and analysis from India, follow WSJ India on Facebook.
Mahindra & Mahindra
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Mahindra & Mahindra's New KUV100 Costs $6,500 in India


क्या कहते हैं आपके सपने? -"मंगनी"
What does your dream mean? -"An Engagement"
अगर मैं सपने मे मंगनी देखूँ तो इसका क्या मतलब है?
What is the meaning of my dream if I see An Engagement ?
if you see An Engagement in your dream it means Delay In Marriage.


text:
Bird On A No Bird Sign
Category: Prose
Published: Thursday, 11 April 2013 13:59
Written by Bart Reckres
"You'll never do it!" jeered Robin, "You'll get yourself killed" mocked Blue Jay "I can't believe you would even think of doing something this stupid" remarked Crow. But Seagull didn't give up, he put his mind to it, and eventually he was on top of the sign. The sign that clearly read "No Birds". This was an enormous risk for Seagull but he landed on it and he stood there. He stood there for almost 20 minutes, Just staring into the distance, waiting for witnesses to this event. A crowd eventually came to be, which included photographers, who took pictures of him, just what Seagull was hoping for, photographers, people who could document this momentous occasion. Never would this happen again, this would be the only time, and this would be the perfect time. There was applause, and everyone loved the bird, they knew he was a very brave bird, you had to be a brave bird to land on a sign that said no birds. Eventually, the image was plastered on people's shirts, hats, and on posters in their houses. Seagull was so excited, he was everywhere, you could not look anywhere without seeing the picture of a bird standing on a sign that said no birds. "I can't believe you did that!" exclaimed Robin, shocked, "I think he cheated" said Blue Jay with displeasure in his voice, "I didn't know you were so fly!" joked Crow. Seagull was the talk of the town. The sign he was standing on was preserved in a museum, which brings thousands of people every week. Seagull was very popular, but unfortunately he tested his luck too much. Since he was so popular he decided he would try another risk, he would fly into a building, hoping to get praise from everybody, he was hoping once the people saw him fly through the window, they would stand up from their seats, applaud and cheer, they would throw roses, they would whistle and they would jump up and down in delight! That had to happen, it happened last time, they would have to recognize him, right? No, that was not the case. He flew in to the building and everybody screamed, jumped out of their seats and ran away, they were so scared because they did not know which seagull it was, since all seagulls look very similar. Seagull felt so stupid, he had never thought of the fact that all seagulls look similar. They threw books at him and he was so confused, eventually he flew away. And was greeted by more jeers by Blue Jay, Robin, and Crow. Seagull was so upset, he went into a dark depression. He was eating three worms a day. He didn't care about anything. He just wanted the jeers to end. Until he thought of a plan. He was going to fly in the museum and go back on the no birds sign. He thought carefully of all of the possibilities of doing the deed, all of the positives and negatives, what time to fly in the museum, what day, what time, he had to factor everything in to make sure nothing wrong happened. He knew he would get more jeers from the birds, but he decided that the deed had to be done. So he took a deep breath and flew through the window, everybody in the museum was confused, Seagull was looking for the sign, but he couldn't find it, he was bumping into walls. Seagull was getting extremely nervous, he was so terrified of not finding the sign, if he didn't find the sign everyone would hate him, and he could be even die from a crazy person from the crowd. But right as he was about to give up, he saw the sign, glowing with a light from the heavens, and he heard a heavenly chorus of Angels signing. He flew up to it and landed on it. Everyone in the museum saw what had happened and cheered. They were jumping up and down with delight, they were throwing roses, they were clapping, they were screaming out of their minds, they could not believe what had just happened, and Seagull had never been more ecstatic. but he had to remain chill, so he would not look like an idiot. He had finally got the respect from before, unfortunately cameras weren't allowed in the museum, so no one could take a picture of the legendary occasion, which kind of disappointed Seagull but he soon realized that it was better if everyone who saw it just knew it by memory. Seagull left, after about 10 minutes of applause, and was greeted again by Blue Jay, Robin, and Crow, who had started to respect him again. "Wow, he did it again!" smirked Blue Jay. "I can't believe this" exclaimed Robin. "Showoff" said Crow. Seagull did not care if his friends were jealous, because he knew, deep down in his heart that he had done a great deed, and that it would follow him to the rest of his life, he didn't care if he would only be remembered for one thing, he would be remembered for something, and that was good enough for him, he would also never try a stupid stunt like flying into a building with nobody knowing what was going on. Seagull can be an inspiration for us, sometimes living life on the edge can give great results. Rules are made to be broken, but you need to know when to stop. If you don't know when to stop, you will be just like the Seagull and lose respect. But if take that one risk, then maybe, just maybe people will remember you, you will be definitely remembered as that one kid who did that one thing. And those memories will certainly last forever.


Many airline workers may be unaware of the potential hazards in their work environment, which makes them more vulnerable to injury. The following references aid in recognizing and controlling hazards that may be present in the airline industry.
FAA Issues Policy to Improve Workplace Safety for Aircraft Cabin Crewmembers. Federal Aviation Administration (FAA) Press Release, August 22, 2013.
Cabin Crew Safety. Flight Safety Foundation (FSF). Links to archives dating back to 1988.
Flight attendants are also responsible for assisting passengers with special needs. See Gate Crew for additional information.
Flight Safety Digest. Flight Safety Foundation (FSF). Addresses general flight and cockpit safety issues.
Please see the OSHA-Airline Ground Safety Panel (AGSP) Alliance page for helpful products pertaining to Ground Crew.
Passengers with Special Needs - Access to the plane and assistance during the flight is a responsibility of the airline and airport.
Access to Air Travel for Disabled Persons and Persons with Reduced Mobility - Code of Practice. United Kingdom Department for Transport (DfT), (July 2008). Provides information about seat allocation, emergency procedure information, catering, assistance dogs, disembarkation, transfer arrangements, and baggage retrieval for the disabled passenger.
Travelers with Disabilities and Medical Conditions. U.S. Department of Homeland Security (DHS), Transportation Security Administration. Describes new security regulations and allowance for prescriptions needed by persons with disabilities and medical conditions.
Policies Regarding Special Needs - Below are some typical policies from selected airlines regarding assisting passengers with disabilities.
Customers with Disabilities. Southwest Airlines.
Mobility and Wheelchair Assistance. Alaska Airlines.
54-Year-Old Certified Electrician Dies in North Carolina. National Institute for Occupational Safety and Health (NIOSH) Fatal Assessment and Control Evaluation (FACE) Program Report 86-47. Reports an incident involving a 54-year-old partner of an electrical contracting company (a certified electrician) who was electrocuted while he repaired airport runway lights. The lights were energized before the task was completed.
Controlling Carbon Monoxide Hazard in Aircraft Refueling Operations. U.S. Department of Health and Human Services (DHHS), National Institute for Occupational Safety and Health (NIOSH) Publication No. 84-106, (February 1984). NIOSH investigators conducted an evaluation of the occupational health hazards of workers who fuel jet aircrafts. Discusses how dangerous concentrations of CO were found in truck cabs where workers spend a considerable amount of time sitting in idling vehicles.
Safe access to aircraft for catering operations. Health and Safety Executive (HSE), (May 2008). Provides guidance for inspectors in preventing falls from height during the catering of aircrafts, and when opening aircraft doors.
Report to Congress: Injuries and Fatalities of Workers Struck by Vehicles on Airport Aprons. U.S. Department of Transportation (DOT), (July 2002). The Wendell H. Ford Aviation Investment and Reform Act for the 21st Century (AIR-21) requires the Federal Aviation Administration (FAA) to study injuries to airport apron workers struck by vehicles and to investigate actions to enhance apron worker safety.
U.S. Army Corps of Engineers Safety and Health Requirements Manual. Electronic Library of Construction Occupational Safety & Health (elcosh), (2003).
Airfield Operations. Provides safety and health requirements for airfield operations.
Baggage Handling: Ramp. OSHA eTool. Addresses hazards associated with plane side loading and unloading using manual, semi-automated, and automated baggage systems.
Ramp Safety. Aviation Safety Reporting System (ASRS) Directline, (June, 1996). Provides an overview of ramp operations and recommendations to avoid ramp operation incidents.
Baggage Handling: Baggage Make-up Room. OSHA eTool. Addresses possible hazards and solutions associated with baggage cart loading and unloading, and general make-up room hazards.
Alaska Airlines Evaluation of Customer Service Agents. State of Washington Department of Labor and Industries, (October 2001). Provides project evaluation of customer service agents (CSAs) for one airline at SeaTac International Airport.


text:
Germany Spending 1 Billion Euros to Dismantle Clean Energy
Washington Post: "Just before midnight on Dec. 31, Germany switched off three more of its nuclear power plants. Once it had 17; now only three are left, and they too will be shut down at the end of the year. Soon Germany will produce no nuclear energy at all. But the activists were wrong to celebrate. Germany's hasty nuclear retreat is neither safe nor green. It's a disastrous mistake that will have ramifications well beyond the country's own borders.
"The Grohnde plant is a perfect example of what Germany is giving up. It was one of the most productive nuclear power plants in the world. It provided enough electricity to cover 15 percent of Lower Saxony's annual energy needs single-handedly, saving 10 million tons of carbon dioxide emissions a year in the process. The site even made headlines in February 2021 for producing more electricity than any other nuclear power plant in the world. Now it will have to be dismantled at a cost of around 1 billion euros."
See also David Frum.
posted by Eugene Wilson | 13sc
The Real Legacy of Fukushima
Washington Post: "A little more than 10 years ago, the world held its breath as Japanese authorities struggled to contain an accident that occurred at the Fukushima Daiichi nuclear power station following a major earthquake. At the time, many observers wondered whether nuclear power, with its radioactive waste and meltdown risk, was worth continuing to use. In retrospect, it was this very backlash — against a virtually carbon-free energy technology that the world needs to slash greenhouse emissions — that turned out to be among the Fukushima saga's most substantial negative consequences."
Tackling Extreme Heat
High Country News: "This summer, Phoenix, Arizona, became the first city in the country to publicly fund an office dedicated to tackling the issue of extreme heat. It's part of a growing awareness among government officials that heat's dangers need to be dealt with more strategically as the world grows warmer. In Phoenix, the nation's third-fastest-warming city, the number of heat-related deaths has continued to climb."
California's Failing Climate Strategy
Wall Street Journal: "'Assuming the same three-year average rate of reduction from 2017 to 2019 (-1.3%), California will reach its 2030 and 2050 goals in 2063 and 2111, respectively,' Next 10 writes. 'Slowing renewable energy growth, underwhelming transportation sector gains, and a worrisome cross-sector over-dependence on natural gas pose major challenges for the state.'"
"Last year the state added more natural gas power capacity than solar. The reason: Fossil fuels are needed to back up unreliable renewables, especially as nuclear power plants are forced to shut down and drought limits hydropower. It also has to import power from other states, some of which is generated by coal."
No Government Would Close Nuclear Plants
David Frum: "No government that really regarded climate change as its top energy priority would close nuclear plants before the end of their useful lives."
Diablo Canyon Plant Extension Economical
John E. Parsons: "We have carefully reviewed CEERT's and PG&E's cost estimates. This analysis strengthens the case made in our original report, that the cost of power from Diablo Canyon Nuclear Power Plant is economical and extending the plant's operating life may offer good value to Californians."
Netherlands' Climate Policy Focused on Nuclear
World Nuclear News: "The Netherlands' new coalition government has placed nuclear power at the heart of its climate and energy policy. Some EUR 500 million (USD 564 million) has been earmarked to support new nuclear build in the period to 2025."
"'We want to make every effort to keep our country and our planet liveable and habitable,' wrote the VVD, D66, CDA and ChristenUnie parties. Today they released the coalition's plans for the period to 2025 as the result of negotiations that began after the general election in March.
"'Nuclear energy can complement solar, wind and geothermal energy in the energy mix and can be used to produce hydrogen,' the document said. 'It also makes us less dependent on gas imports.'"
Conservative Climate Caucus
Nuclear Newswire: "The environmental benefit of nuclear has support across political divides. Recently, a third of all House Republicans launched the Conservative Climate Caucus. Its head, Rep. John Curtis (R., Utah), gave an interview. When he was asked about ideas for solving climate change, he gave only one specific policy: 'We can do nuclear at large scale and without a carbon footprint.'"
Nuclear Energy's Track Record
The Breakthrough Institute: "What has been clear, from the beginning of the nuclear era is that when nations decide that they want or need nuclear energy, they can and have repeatedly taken steps to put programs and regulations in effect that allow them to have it, safely and at a reasonable cost. This has been true in France, Korea, Japan, even Germany, and today in China."
Desalination at Diablo Canyon Could Provide Very Significant Drought Relief
MIT News: "The cost of desalinated water produced at Diablo Canyon would be lower than for a stand-alone plant because the cost of electricity would be significantly lower and you could take advantage of the existing infrastructure for the intake of seawater and the outfall of brine. Electricity would be cheaper because the location takes advantage of Diablo Canyon's unique capability to provide low cost, zero-carbon baseload power."
"Depending on the scale at which the desalination plant is built, you could make a very significant impact on the water shortfalls of state and federal projects in the area. In fact, one of the numbers that came out of this study was that an intermediate-sized desalination plant there would produce more fresh water than the highest estimate of the net yield from the proposed Delta Conveyance Project on the Sacramento River. You could get that amount of water at Diablo Canyon for an investment cost less than half as large, and without the associated impacts that would come with the Delta Conveyance Project."


Is It Worth Putting Your Job at Risk for $25?
Personalized Direct Mail, Theory or Reality?
CNN Video: How much do stamps cost again?
Why Did Federal Prosecutors Drop Their Lance Armstrong Case?
Local union president says USPS hiring is "smoke and mirrors"
Remember! Stamp prices go up Sunday!
USPS issues Vermont Covered Bridge stamp- in Georgia?
USPS Sends Priority Mail Package 1,688 Miles Out Of Its Way?
How Will the January 2013 USPS Postage Hike Impact You?
Why did the U.S. Postal Service sponsor a cycling team?
Stop the Madness! The U.S. Postal Service Is Not Going To Die!
PM says he's concerned "about how some employees there might react the day the center shuts down"
Columnist: Remind me again- why did the USPS sponsor Lance?
"... his potential problems with the Postal Service are in a class of their own..."
USPS has booth at Consumer Electronics Show?? Featuring Marilyn Monroe????
Video: Massive Cuts to Postal Service a Step Towards Privatization?
Why do city carriers get tons of Xmas OT and rurals don't?
Ask The Experts: Is my USPS pension safe?
Will House Republicans Let The Post Office Save Itself This Year?
"The Postal Service should not have to do business this way"
What's that old saying about "good intentions"?
Ridiculous Overtime at the USPS in 2013?


The DIARY directory platform provides fashion, beauty and lifestyle industry news, interviews, dates, vacancies and contacts. Our huge database of contacts includes thousands of digital influencers, media titles (UK and overseas) and their editorial teams, freelance journalists and creatives, PRs and brands and representative agencies. Live and sortable social media stats for entries allow comparative analysis and insight within filtered sections.


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Facebook mulling policy changes on gun-themed pages (exclusive)
Richard Byrne Reilly	 March 3, 2014 4:00 PM
Facebook may announce company policy changes for gun-related pages in mere days, VentureBeat has learned.
The social network has been under pressure from the powerful Mayors Against Illegal Guns and the Moms Demand Action civic group to ban gun-themed fan pages on the site.
"Talks are progressing. The discussions are ongoing; there have been positive developments," sources close to the conversations told VentureBeat.
An extensive VentureBeat investigation last week revealed that adults and children were making arrangements to buy, sell, and trade guns through the many Facebook fan pages devoted to guns and the people who use them, sometimes in violation of federal and state gun laws.
Last October, a 15-year-old high school student in Kentucky bought a 9mm handgun from a man he met through a Facebook fan page. The teen was arrested when he was caught with the loaded pistol on the campus of Greenup County High School. The seller drove from Ohio to Kentucky to make the sale and was also arrested. The suspect told sheriff's investigators he sold other guns to people he met on Facebook fan pages.
The two advocacy groups recently joined forces to pressure "Facebook [to] get out of the gun business." Mayors Against Illegal Guns was cofounded by former NYC three-term mayor and billionaire Michael Bloomberg along with Boston's then-mayor, Thomas Menino, in 2006. Mayors of more than 1,100 U.S. cities belong to the organization.
A Moms Demand Action petition on Change.org to prohibit gun sales on Facebook and Facebook-owned Instagram has over 94,000 signatures. Comedian Sarah Silverman recently tweeted about the campaign, which is getting massive exposure through U.S. media outlets.
The petition is addressed to Instagram chief executive Kevin Systrom and Facebook cofounder and chief executive Mark Zuckerberg:
Mark Zuckerberg, Facebook CEO
Kevin Systrom, Instagram CEO
Your platforms unfortunately allow users to buy, sell, and trade firearms without requiring criminal background checks.Other online platforms including Craigslist, eBay, and Google+ have already prohibited these sales.I ask that you put an end to this completely unregulated social media gun show and prohibit gun sales from your platforms immediately.
"Anybody can go to Facebook and Instagram and buy a gun online. We're asking them to review their policies," a spokeswoman for Mayors Against Illegal Guns told VentureBeat last week.
Facebook, of course, is not an e-commerce site and doesn't sell anything. Last week, a Facebook spokesperson told VentureBeat, "You can't buy things on Instagram and Facebook, nor can you promote the sale or use of weapons in advertising. We encourage people who come across any illegal activity to report it to us."
Users are still getting around the company's stated user policies.
Google+, with about 450 millions users, also prohibits the sale of guns and many other items through the site.
A Facebook spokesperson declined to comment Monday.
Federal law enforcement sources told VentureBeat they view Facebook, Instagram, and other social media platforms "as emerging threats for unlawful gun transactions in the United States."


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Conopsia flavimacula is een vlinder uit de familie wespvlinders (Sesiidae), onderfamilie Tinthiinae.

Conopsia flavimacula is voor het eerst wetenschappelijk beschreven door Kallies in 2000. De soort komt voor in het Afrotropisch gebied.

Wespvlinders
Dier uit het Afrotropisch gebied

redpajama_set_name: RedPajamaWikipedia


text:
Salem cook ready for World Food Championships
The World Food Championships is the largest competition in food sport, where champions of previous events convene in Kissimmee, Florida, for a chance at winning the ultimate food crown and a share of $300,000. In three short years, WFC has awarded more than $1 million in prizes and money, spawned a TV series, garnered more than 5 billion media impressions and launched numerous professional careers for successful contestants, according to the contest.
This time, Banick will have two assistants traveling with her, Kasey Brown, a professional baker who formerly had her own business, and her husband, Mark Banick.
"I'm just going to do whatever she needs me to do," he said.
he team will cook all day on Nov. 7. They'll prepare a traditional red chili called Graham's Red Chili, a beef chili with no beans, followed by a tailgate-themed chili called Adam's Rib and the Bad Apple that has to include Hormel no bean chili. And then the team will have to compete in the People's Choice Chili Fest, where they are making three gallons of their tailgate-themed chili, which uses Adam's Rib barbecue sauce and 2 Towns Cider Bad Apple, two of her sponsors. Tasters pay $15 to attend the People's Choice Chili Fest and get five tasting cups and spoons and one token to vote for their favorite chili, Banick said.
4 delicious gluten-free recipes from West Salem cook
There are 26 total competitors in the chili division, so Banick will be facing stiff competition. The top winners advance to the next stage of the competition, a freestyle chili cookoff, where Banick will be making an elk chili that uses wine from Willamette Valley Vineyards, one of her sponsors. The chili will be served in custom-made Willamette Valley Vineyards wine bottle bowls made for her by McMinnville resident Graham Rankin.
Banick said she qualified for the event by wining the grand prize in the Hormel Chili Contest back in April and won a Golden Ticket to attend the competition, along with travel stipend.
Banick said she's been spending at least two months practicing.
"I really don't want to eat chili for a while after this," she said.
Follow Kim
Follow Kim Banick's progress at the World Food Championships on her blog at theprizeofcooking.com and on her Facebook page, Facebook.com/kim.banick.


Spring is in the air! The smell of freshly cut grass, bees a buzzing and the birds doing their thing … let the super-mellow 'Sweet Pea' by Jem Stone sooth your mind and take you on a 10 minute journey. Like floating in a mellow dream, you won't want to wake up…..


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One Man
PGPG
DramaThriller
A crusading TV reporter finds his life ripped apart as he investigates a story about a company's deadly criminal negligence.A crusading TV reporter finds his life ripped apart as he investigates a story about a company's deadly criminal negligence.A crusading TV reporter finds his life ripped apart as he investigates a story about a company's deadly criminal negligence.
Robin Spry
Robin Spry(screenplay by)
Peter Pearson(screenplay by)
Peter Madden(screenplay by)
Len Cariou
Jayne Eastwood
Carol Lazare
2 wins & 3 nominations
Jason Brady
Alicia Brady
Marion Galbraith
Colin Angus Campbell
August Schellenberg
Ernie Carrick
Jean Lapointe
Ben Legault
Sean Sullivan
Rodney Porter
Terry Haig
Dr. Gendron
Marc Legault
Danny Freedman
First Hood
Second Hood
Robert V. Girolami
John - TV Announcer
(as Bob Girolami)
Jacques Godin
Donovan Hare
Donovan Brady
Kevin Hare
Jesse Brown
Nang Brady
Peter MacNeill
Michel Maillot
Robin Spry(screenplay by) (from an original idea by)
A Little Night Music
Evil Judgment
L'eau chaude, l'eau frette
The Apple, the Stem and the Seeds!
Drying Up the Streets
Les chats bottés
Une jeune fille à la fenêtre
Ti-mine, Bernie pis la gang...
O.K. ... Laliberté
Len Cariou's film debut.
A narrator recounts a list of specific incidents relating to industrial chemical pollution causing death all over the world.
A Politically Oriented Enviro-Thriller With An Ending Inspired By Cronenberg.
A TV reporter from Montreal, known for covering gang violence, happens upon a story about numerous children being poisoned by a chemical called benzo(a)pyrene or b.a.p.
The woman who puts him on to the story tracks the source of the chemical to a company called Konrad's, an industrial operation that suffered a leak of the toxic substance which also killed at least one of it's workers.
His investigations have him stepping on a lot of toes, leaving him to deal with corrupt cops, the mob, a jealous wife, and, now, a cabal of union goons who work for the chemical company.
He does his best to get the story on the air, but is stifled at every turn.
As a result of threats to his family and friends, the promise that Konrad's parent company will pull advertising from the TV station he works for in an attempt to make them lose revenue and force them into bankruptcy, and by ruining the credibility of those around him.
He almost gives in to this duress, but knows he wouldn't be able to live with himself if he sold out in order to protect the interests of those responsible.
So, even when he loses his family, and his best friend is murdered, he refuses to give in and let them silence him.
Interestingly, this all culminates in a finale that is incredibly similar to Cronenberg's Shivers...only, instead of parasite infested sex zombies, he finds himself surrounded by a group of angry union workers who aren't willing to give up their jobs for the benefit of the community at large.
In both cases, the lone remaining individual is forced to decide whether he is going to take a stand, and be ostracized- or worse- for it, or give in and conform to the demands of the angry masses, simply in order to survive and be accepted.
Unlike, shivers, however...we get to see how this all plays out.
It does seem like director Robin Spry was directly influenced by Cronenberg's film, which had come out only two years prior (being the highest grossing Canadian feature film at the time), and was also shot in Montreal.
Either way, however, the parallels are there.
In the end, though lacking a well developed plot structure, this film really is quite interesting.
A politically oriented, environmental thriller, set amidst an urban environment.
And kind of middle ground between Steven Soderbergh's Erin Brockovich and Michael Moore's Canadian Bacon (less the comedy angle).
5.5 out of 10.
meddlecore
July 1979 (United States)
Einer allein
National Film Board of Canada (NFB)
CA$350,000 (estimated)
By what name was One Man (1977) officially released in Canada in English?


CLEAR PLASTIC STAND: LHE-46 is yet another addition to Clear-Ad's range of acrylic office products. The three sided tent style display stand is made with clear plastic with excellent visibility. The triangular tower shaped stand is designed for counter and table tops.
UNBREAKABLE MENU HOLDER: The menu holder is constructed with thick and clear as glass premium acrylic plastic sheet that look and feel exactly like glass but is unbreakable and lasts much longer than glass. There are no imperfections or distortions to affect visibility.
STURDY TABLE TOP DISPLAY STAND: The display case is designed to stand on table and counter tops. The triangular design affords great visibility of your advertisement and can be firmly placed on any flat surface without toppling over.
LARGE PHOTO FRAME: The table tent can be used to display large photographs, advertisements, menus, information or notices. They are ideal for homes, offices, restaurants, canteens, schools, etc. The equilateral prism shape affords maximum viewing with minimum effort. It can be used in both portrait and landscape format.
SINGLE SHEET CONSTRUCTION: Each LHE-46 is made with a single sheet of premium grade acrylic. The sheet is laser cut and heat bonded to shape into the desired shape. The three sided display stand is open at the bottom and along the sides to insert the pamphlet.
Clear-Ad is known for its clear acrylic office and business products. The LHE-46 is another premium product in its clear acrylic range of products which include all kinds of office products, stands and display sleeves for promotional material. The three sided display stand is ideal to be placed on flat surfaces and can be viewed easily from all the sides. Keep your promotional material safe and clearly visible.
LHE-46 can hold 4 x 6 inch sheet on each of its size. Any flyer, postcard, or any other promotional material of that size can be displayed with this stand. Each of the three sides have separate sleeves which provide you with the opportunity of displaying three different messages as one time.
Each table tent is created with premium grade acrylic sheets. Each sheet is precision cut and heat molded and bonded to create a strong and sturdy product that is designed to give you years of great service. Each stand is created from a single sheet and is thus very strong and durable. The acrylic is clear affording great visibility and is very tough. It will not break or crack if it falls. Each side contains a pamphlet sleeve that is open around the sides and at the bottom. The display sheet can be loaded from the bottom and stays in place wedged between the precision molded surfaces of the sleeve.
Get you message across clearly. Buy the pack of 40 NOW.


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The Newly Built Printing Press at the Headquarters Has Been Officially Handed Over to the University.
The edifice was constructed by FIK Engineering, Abuja.
The company's project engineer, Mike Olukotun, who took the officials representing the university, the consultant as well as other stakeholders round the building; said it took the company just 8 months to finish the work.
Mr Olukotun said the building has a printing press in two wings, computer rooms, offices for staff, production room and stores.
He thanked the management for the full cooperation, saying they encountered no hitch whatsoever during the period.
The DPDW&S director, was represented by a team from the directorate in receiving the new building.
They were led by a Principal Architect, Enyinnaya Akueshi, who alongside the consultant, pointed minor observations that would be effected within a fortnight.
Important Notice: Faculty of Management Sciences ENT210 & ENT312
NOUN TMA Questions and Answers: ECO718 – Macro-Economic Theory I


FORTUNE — Last week brought reports of a deal to chop as much as a decade off the prison term of Jeff Skilling, the former Enron CEO and convicted fraudster. But the real reason for the dramatic sentence reduction is different than some of the media coverage has suggested.
With credit for good time and a drug and alcohol program, Skilling, who is 59 and has served six years already, could get another two and a half years off, freeing him from prison by his mid-60s. The deal will also release more than $40 million in assets seized from Skilling, to be distributed to Enron's financial victims, and will require him to abandon his appeals.
The bulk of the proposed sentence reduction, however, results not from last week's negotiated agreement between the government and defense lawyers, but from a 2009 decision by the Fifth Circuit Court of Appeals.
Knowing the real story eliminates the prospect that the defense had some powerful new card to play, such as prosecutorial misconduct — and suggests that it was instead simply a matter of both sides seeking closure.
Here's what happened. Skilling was originally convicted in May 2006, after a four-month trial. (Former Enron chairman Kenneth Lay was also convicted, but died of a heart attack six weeks later.) Under federal sentencing guidelines, which use a points system, Skilling's offenses and background put him at a level 36. Judge Lake added a four-level "enhancement" for jeopardizing the safety and soundness of a "financial institution." This aggressive ruling — which defined Enron's employee retirement plans as a "financial institution" — boosted his level to 40, with a range of 292 to 365 months. Lake's sentence of 24 years and four months was at the minimum of that guideline.
In a January 2009 decision, the Fifth Circuit upheld Skilling's conviction, but threw out the "financial institution" enhancement, cutting his number back down to 36, with a range of 188 to 235 months — or as little as 15 years and eight months. The appeals court ordered that he be resentenced.
But that resentencing was postponed indefinitely pending more Skilling appeals, which included two trips to the Supreme Court (which declined to overturn his conviction), and another round before the court of appeals. Negotiations began in earnest after Skilling's prospects for overturning his conviction grew dim.
The agreement announced last week trims his sentencing number just one more level, to a range of 168 to 210 months. If sentenced again at the bottom of the range, this would produce a further reduction of one year and eight months, to 14 years. The resentencing is scheduled for June 21 in Houston.


The RSC 'continues its commitment to semi-integrated British sign language performances' where interpreters appear on stage with the actors, dressed as appropriate characters.
This was its announcement for Midsummer Night's Dream last summer, which followed on from the success of the technique in its production of the Christmas Truce on 2015. The technique has been introduced by Erica Whyman, now Depute Artistic Director with the RSC, and formerly with Northern Stage, Newcastle upon Tyne, where integrated signed performances were also part of the access strategy for audience with special needs.
I have good reason to believe that the RSC is committed to continuing its access to deaf children and adults. More of this anon….


text:
Website: See below
Survive is a full cast audio drama series about a group of Canadian survivors of a zombie apocalypse. The audio drama is inspired by the graphic novel and television series The Walking Dead. Episodes are available as streaming YouTube videos.
No longer dealing with hypotheticals, the outbreak has finally happened! Follow a group of survivors as they trudge through a wasteland which was once a great British Columbia park, in search of anything to aid in their survival.
Part 1 YouTube video
full cast, horror, mature content, sound effects, streaming
full cast horror mature content sound effects streaming