text:
\section{Introduction}

The propagation of shock waves is an ubiquitous phenomenon in the interstellar medium, where the sound speed is low due to the temperature conditions. Observations over the past few decades (\citealt{Snell80}) have shown that, at the early stages of the formation of solar-type stars,  the process of mass accretion is almost always associated with mass ejection, in the form of collimated jets, extending from a few astronomical units up to parsecs from the exciting source (\citealt{Dougados00,Bally96}). The supersonic impact between the jet and the parent cloud generates a shock front, which propagates in the collapsing interstellar gas, and also an inverse shock that propagates along the jet itself. Large cavities, called bipolar outflows, appear, which have been extensively studied through the molecular emission that they generate (\citealt{Bachiller96}). At the apices of these cavities, the shock wave heats, compresses and accelerates the ambient interstellar gas. As the temperature rises to at least a few thousands degrees, the energy barriers of numerous reactions involving neutral or ionized molecules can be overcome and the chemistry of certain species can be significantly altered (\citealt{Bachiller01}). Similarly, processes specific to the propagation of shock waves affect the interstellar grains (\citealt{Flower031,Guillet07,Guillet09}), leading to the injection of molecular and atomic species into the gas phase, such as silicon-bearing species (\citealt{Schilke97,Gusdorf081}, hereafter G08a). The time-scales involved in the heating and in some of the shock chemical processes are short (10$^2$ to 10$^4$ years; \citealt{Gusdorf082}, hereafter G08b), so the shocked region rapidly acquires a chemical composition distinct from that of the quiescent medium. As the gas cools down radiatively, reactions with high energy barriers no longer operate, and the chemistry is dominated again by low-temperature reactions. The resulting molecular emission can be used as a diagnostic tool to study the physical and chemical characteristics of the shocked region.

Recently, G08b placed constraints on shock parameters using H$_2$, SiO and CO observations in the B1 knot of the L1157 outflow. At the same time, the HIFI and PACS receivers on \textit{Herschel} have observed the entire L1157 outflow (\citealt{Nisini10}) and provided velocity-resolved data of the L1157-B1 knot (\citealt{Lefloch10,Codella10}). Their studies indicate that the H$_2$, SiO and H$_2$O emission regions are spatially coincident on large scales. They also shed light on the necessity to provide reliable models of water emission in order to better understand its production in shocks and its role in the cooling of the outflow. Recently, \citet{Flower10} (hereafter FP10) presented an extensive study of water emission for a small grid of stationary shock models, and compared it to \textit{Spitzer} observations of water emission in NGC2071, with a certain level of agreement. Our aim is to push the confrontation between models and observations one step further, by using the models, which have already demonstrated their ability to reproduce some observations, to predict water line intensities. Using an approach to comparing models with observations that is similar to that of G08b, as applied to H$_2$ and SiO, we aim to constrain the physical and chemical parameters of the targeted region. In a second step, we incorporate these preliminary constraints and the latest compilation of molecular data for H$_2$O in an LVG radiative transfer code to provide predictions of water emission, under the assumption that the emission regions of the various species coincide.

The choice of target is of crucial importance, as our candidate must have been the object of prior studies, and must be a good potential target for contemporary and future instruments such as \textit{Herschel} and ALMA. Located at a distance of about 175 pc, the Bok globule BHR71 (\citealt{Bourke95}) is a well-known example of isolated star formation observable in the southern hemisphere, and hence is a reasonable candidate for future ALMA observations. Its observation by the \textit{Herschel} telescope is guaranteed through the key-program WISH, and also DIGIT. The associated outflow region contains signatures of two distinct molecular jets (\citealt{Bourke97,Myers98,Parise06}) centered on two different protostellar sources, IRS1 and IRS2 (\citealt{Bourke012}) separated by $\sim$3400~AU. Bright HH objects are associated with the blue-shifted lobes of each outflow, HH320 and HH321 (\citealt{Corporon97}). They have been imaged in the \ion{S}{ii} transition at 6711~\AA, indicating that at least part of the outflows are dissociative. The dynamical age of HH321 is estimated to be 400~years (\citealt{Corporon97}). It has not yet been possible to determine the dynamical age for HH320. NIR JHK-band spectra covering both HH320 and HH321 were obtained by \citet{Giannini04}. Through detailed shock modelling they derived a pre-shock density of 10$^4$~cm$^{-3}$ and shock velocity of 41~km/s for HH320A; this was found by fitting a non-steady-state shock model to the observed H$_2$ lines. The age of the non-steady-state shock is 475~years, which is more or less in agreement with the dynamical age of the HH321 flow. The  pre-shock density is lower than is predicted on the basis of CO observations, 10$^5$~cm$^{-3}$ (\citealt{Parise06}). However, the latter is the density of the molecular outflow, which is compressed relative to the ambient pre-shock cloud. These inner parts of the bipolar outflow, covering the HH objects, have also been targeted by the  \textit{Spitzer} Space Telescope, and the corresponding results in terms of rotational H$_2$ excitation diagrams have been made available by \citet{Neufeld09}. Another article is dedicated to the parameters map analysis based on these data (\citealt{Giannini11}). Finally, \citet{Garay98} have presented maps of SiO~(2--1) and (3--2) of the whole bipolar outflow.

In Section~\ref{sec:h2oam}, we presented a combined analysis of both rovibrational transitions of H$_2$ from \citet{Giannini04} and rotational lines, as compiled by \textit{Spitzer} (\citealt{Neufeld09}). We then briefly present the code that is used to simulate the propagation of shock waves through the interstellar medium, and introduce the grid of models that we computed. Finally we describe the constraints that we obtain in several knots of the BHR71 outflow by comparing more or less complete H$_2$ observations with models. In Section~\ref{sec:SiOoam}, we present the results of comparisons between observations of SiO and the models. We describe the observing setups, the actual observations, and the results in terms of simultaneous fits of the H$_2$ and SiO molecules. Section~\ref{sec:wep} contains our predictions of water emission line intensities. We briefly summarize our methodology and then discuss the appropriateness of the steady-state and statistical equilibrium assumptions, before presenting a comparison of results obtained using each of these approximations. Section~\ref{sec:cr} contains our concluding remarks.

\section{H$_2$ observations and modelling}
\label{sec:h2oam}

\subsection{Observations}
\label{sub:h2o}

There are two distinct sets of H$_2$ observations. The details of the ground-based observations of the rovibrational transitions are reported in \citet{Giannini04}. The \textit{Spitzer} observations of the pure rotational transitions, described in \citet{Neufeld09}, are the subject of an separate article (\citealt{Giannini11}).

The comparison between observations of H$_2$ emission and model results is usually based on excitation diagrams that are derived for selected emission regions. Such excitation diagrams display ln($N_{vj}/g_j$) as a function of $E_{vj}/k_{\rm B}$, where $N_{vj}$ (cm$^{-2}$) is the column density of the rovibrational level ($v, J$), $E_{vj}/k_{\rm B}$ is its excitation energy (in K), and $g_j = (2j+1)(2I+1)$ its statistical weight (with $I=1$ and $I=0$ in the respective cases of ortho- and para-H$_2$). If the gas is thermalized at a single temperature, all the points in the diagram fall on a straight~line.

\begin{table}
\caption{The considered positions in the BHR71 outflow.}
\label{table1}
\centering
\begin{tabular}{c c c}
\hline
position name & R. A. (J2000)  & Decl. (J2000)  \\
\hline \hline
   central position & 12$^{\rm h}$01$^{\rm m}$36 \fs 07 & $-$65$^\circ$08$'$50 \farcs 5 \\
   IRS1 & 12$^{\rm h}$01$^{\rm m}$36 \fs 63 & $-$65$^\circ$08$'$48 \farcs 5 \\
   IRS2 & 12$^{\rm h}$01$^{\rm m}$34 \fs 00 & $-$65$^\circ$08$'$44 \farcs 5 \\
   HH320AB & 12$^{\rm h}$01$^{\rm m}$31 \fs 20 & $-$65$^\circ$08$'$05 \farcs 0 \\
   HH321AB & 12$^{\rm h}$01$^{\rm m}$36 \fs 70 & $-$65$^\circ$09$'$32 \farcs 0 \\
   knot 5 & 12$^{\rm h}$01$^{\rm m}$32 \fs 60 & $-$65$^\circ$08$'$23 \farcs 3 \\
   knot 6 & 12$^{\rm h}$01$^{\rm m}$36 \fs 00 & $-$65$^\circ$09$'$18 \farcs 6 \\
   knot 8 & 12$^{\rm h}$01$^{\rm m}$38 \fs 90 & $-$65$^\circ$10$'$07 \farcs 0 \\
   SiO peak & 12$^{\rm h}$01$^{\rm m}$33 \fs 80 & $-$65$^\circ$07$'$24 \farcs 0 \\
   SiO knot & 12$^{\rm h}$01$^{\rm m}$36 \fs 00 & $-$65$^\circ$07$'$34 \farcs 0 \\
\hline
\end{tabular}
\end{table}

In their original study of conditions in the BHR71 outflow, \citet{Giannini04} extracted the excitation diagrams corresponding to nine positions (knots 1 to 9) and four HH objects (HH320A\slash B and HH321A\slash B), in order to compare their observations with shock models. In the present study, we attempt to make use of most of the available data, both in the pure rotational and in the rovibrational transitions of molecular hydrogen. Unfortunately, combining the two sets of observations is only possible where both sets of data are available and when a cross calibration can be performed to ensure their consistency. We consequently make use of the following excitation diagrams~:
\begin{itemize}
\item pure rotational transitions for the \lq H$_2$ knots' 5, 6, 8 as denoted by \citet{Giannini04}~;
\item rotational and rovibrational transitions for the two Herbig-Haro objects that are called HH320AB and HH321AB, as defined by \citet{Giannini11}~;
\item pure rotational transitions on the \lq SiO knot' (see Subsection~\ref{sub:SiOr}).
\end{itemize}

   \begin{figure}
   \centering
   \includegraphics[height=9cm,angle=-90]{16758fg1.eps}
      \caption{The internal parts of the BHR71 outflow as observed by \textit{Spitzer} in the H$_2$ 0--0 S(5) transition (\citealt{Neufeld09}); the colour scale unit is erg~cm$^{-2}$~s$^{-1}$~sr$^{-1}$. The contours correspond to the levels of 3, 9, 15, 21, 27, and 33~$\sigma$. The pink hexagons give the positions of the IRS1 and IRS2 sources as determined by \citet{Bourke01}. The positions of the Herbig-Haro objects HH320AB and HH321AB are plotted in black as well as those of the SiO peak (referring to the point of maximum SiO~(5--4) emission, see Section~\ref{sec:SiOoam}), and of the SiO knot, which was chosen to perform our simultaneous fit of H$_2$ and SiO emission, and also to make predictions of water emission. The other emission knots that were analysed are plotted in white (knots 5, 6, and 8, following the labelling of  \citealt{Giannini04}). Around the SiO-peak, four radii are displayed, corresponding to 5, 9, 12, and 14.4$''$. The first represents the size of our region of analysis. The latter three correspond to the beam of the APEX telescope for the SiO (8-7), (6-5) and (5-4) transitions, respectively; see text.}
         \label{figure1}
   \end{figure}

The corresponding list of coordinates is provided in Table~\ref{table1}. All these points are presented in Figure~\ref{figure1}, which shows the internal parts of the BHR71 outflow, as mapped by the \textit{Spitzer} Space Telescope in the 0--0~S(5) spectral line of H$_2$ (\citealt{Neufeld09}). In each case, the excitation diagrams were extracted for a circular emission region of 5$''$ radius, centered on these positions, shown for the case of the so-called \lq SiO peak' (see Subsection~\ref{sub:SiOr}) in Figure~\ref{figure1} (smallest circle). In the case of the Herbig-Haro objects, the consistency between the rotational and rovibrational data sets was ensured by means of the following method, as explained by \citet{Giannini11}. First, the image of H$_2$ 1--0 S(1) line at 2.122~$\mu$m (retrieved from the ESO archive at http://archive.eso.org/eso/eso\_archive\_main.html) is degraded to the \textit{Spitzer} spatial resolution of 2$^{\prime\prime}$/px. Then, this image is calibrated by using 2MASS fluxes of several bright stars in the field, and the photometry is computed in the same areas of 5$^{\prime\prime}$ radius as the \textit{Spitzer} images. To find the intercalibration factor between imaging and spectroscopy, the measured 2.12~$\mu$m flux was compared with the flux measured in the 1$^{\prime\prime}$ slit where spectroscopic observations have been performed. Finally, the same factor was applied to the fluxes of the other NIR lines, adopting averages of the line ratios (relative to the 2.12~$\mu$m transition) in the A and B substructures of HH320 and HH321.

The data were corrected for extinction, adopting the upper limit of the visual extinction from \citet{Giannini04}, $A_{\rm V} = 2$, and using the interstellar extinction law of \citet{Rieke85}. We note that the effect of the interstellar extinction on the observational points is minor. The excitation diagrams resulting from the observations are plotted in Figure~\ref{Figure2}. The rotational and rovibrational temperatures derived from these observations are also indicated on the plots in the same colour code, along with the corresponding line. Again, the reddening correction has only minor significance on the temperature values. As anticipated, the rovibrational transitions are found to trace warmer gas than the pure rotational transitions (see, for example, \citealt{Lebourlot02, Giannini06}, and G08b).

   \begin{figure*}
   \centering
   \includegraphics[width=18cm]{16758fg2.eps}
      \caption{The H$_2$ excitation diagrams observed for each position indicated in Figure~\ref{figure1}, in black (pure rotational lines), and grey (rovibrational lines, when available). The data were corrected for extinction, using A$_{\rm V}=2$ from \citet{Giannini04}. The inferred rotational temperatures are indicated in black, and the rovibrational temperatures, in grey. The best-fitting model results are also shown in each case, in blue and/or red symbols. The shock parameters are given in each panel in the corresponding colour.}
         \label{Figure2}
   \end{figure*}

\subsection{Grid of models}
\label{sub:gom}

\begin{table}
\caption{Input parameters of our grid of stationary C- and non-stationary CJ-type shock models.}
\label{table2}
\centering
\begin{tabular}{c c c c}
\hline
type & $n_{\rm H}$ (cm$^{-3}$) & b & $\varv_{\rm s}$ (km s$^{-1}$)  \\
\hline \hline
C & 10$^4$ & $\in$ [0.45 ; 2] & \tiny{10,15,20,22,25,28,30,32,35,55} \\
C & 10$^5$ & $\in$ [0.30 ; 2] & \tiny{10,12,15,18,20,40} \\
C & 10$^6$ & 1 & \tiny{10,12,15,18,20,22,25,27,30,32} \\
\hline
CJ & 10$^4$ & $\in$ [0.45 ; 2] & \tiny{10,12,15,20,22, 25,28,30,32,35} \\
CJ & 10$^5$ & $\in$ [0.30 ; 2] & \tiny{10,12,15,18,20} \\
\hline
\end{tabular}
\end{table}

The shock code that we use to simulate the propagation of shock waves in the interstellar medium is described in G08b. It generates one-dimensional stationary models of both continuous or discontinuous kind (respectively, C- or J- type shocks), and also approximations to time-dependent solutions, in the form of a shock wave possessing the characteristics of both C- and J-type models (see \citealt{Chieze98,Lesaffre041,Lesaffre042}). The shock code solves the differential equations that determine the evolution of a set of dynamical and chemical variables: the neutral and ionized fluid temperatures, velocities and densities; the fractional abundances of over 125 species, linked by more than 1000 chemical reactions. The populations of the first 150 levels of molecular hydrogen are calculated within the shock code, based on the treatment of  \citet{Lebourlot02}, with the only difference being that we adopted the most recent H--H$_2$ collisional rate coefficients (\citealt{Wrathmall07}). Finally, grain-related processes are also included in the code, following \citet{Flower031}.

The parameters that we aim to constrain are the inputs of the models, namely:
\begin{itemize}
\item ambient-medium-related quantities: pre-shock density $n_{\rm H}$ and magnetic-field parameter $b$, defined by B($\mu$G)~=~$b~\times~\sqrt{n_{\rm H}~({\rm cm}^{-3})} $;
\item shock-related quantities: shock velocity $\varv_{\rm s}$, and age in the case of a non-stationary solution;
\item chemistry-related quantities, such as the initial value of the ortho-para ratio for molecular hydrogen, or the initial distribution of silicon-bearing material in the grains.
\end{itemize}

As a first step, we made use of a grid of stationary C-type shock models with the parameters specified in Table~\ref{table2}. We should mention that the parameter coverage is not complete, in the sense that not all velocities are present in our grid for all values of the magnetic-field parameter, $b$. In fact, the velocity of C-type shocks must remain below a critical value that depends mainly on the pre-shock density and magnetic-field parameter (\citealt{Lebourlot02,Flower031}), which explains the decrease of the maximum shock velocity with the pre-shock density in our grid. Following the method presented in G08b (Section~4.1), this set of C-type shock models enabled us to restrict the range of the search in the parameter space for the CJ-type shock models. We then computed a grid of non-stationary shock models around a first estimate of the shock age, making sure that the range of ages was sufficient to include any model likely to fit the H$_2$ observational data. The grid of CJ-type models covers the combination of parameters given in Table~\ref{table2}, for ages ranging from a few tens to a few thousands of years.

For each of the above models, we obtained an excitation diagram that can be compared with observations.

\subsection{Comparisons and initial constraints}
\label{sub:cafc}

We describe here the results of the comparisons between observations and our models. A few preliminary remarks about our results are applicable to all the knots and regions analysed. First, the filling factor was considered to be equal to 1 for all transitions; this yields H$_2$ knot sizes consistent with the thickness of the H$_2$ emitting layer of our models. Secondly, under this assumption, we find that, in all cases, only non-stationary shock models reproduce satisfactorily both the pure rotational and rovibrational (when available) parts of the H$_2$ excitation diagram, a result that has already been established in similar studies of other objects (e.g. HH54, \citealt{Giannini06}, or L1157-B1, see G08b). Finally, the departure of the observational points from a straight line in the purely rotational parts of the excitation diagram (\lq saw-tooth' pattern, which is weak in our cases) is indicative of deviations of the ortho-to-para ratio from the high-temperature LTE value of 3.0. Such a pattern can be reproduced in the models by slightly modifying the value of the initial ortho-to-para ratio; but fine-tuning this parameter is not a major consideration in the context of the present study.

We give prior focus to the Herbig-Haro objects, for which we can benefit from H$_2$ excitation diagrams combining pure rotational and rovibrational transitions, and to the so-called \lq SiO knot', for which future observations of SiO rotational transitions are expected to provide further constraints on our shock models. Tables~\ref{tablea1} and \ref{tablea2} present a summary of the restrictions that comparisons between observational and computed excitation diagrams place on the shock model parameters. In these tables, the values of the pre-shock density, magnetic-field parameter and shock velocity are indicated for our best models, as well as the age range for which the excitation diagrams are in satisfactory lagreement with the observations. In the case of the Herbig-Haro objects HH320A\slash B and HH321A\slash B, the best-fitting models are non-stationary, and the pre-shock density is constrained to 10$^4$~cm$^{-3}$, which is in agreement with the average density of the whole globule (9$\times$10$^{3}$~cm$^{-3}$), as determined by \citet{Bourke97}. Shock velocities in the range 15--35~km~s$^{-1}$ yield good fits to the observations, depending on the associated magnetic-field parameter and age. We note that the shock ages that we obtain are of the same order of magnitude as the observational dynamical ages. The excitation conditions are remarkably similar in both sources, in spite of their location on a different lobe of the outflow, and the probable mixing of the two outflows from IRS1 and IRS2. In the case of HH320A\slash B, our findings are in agreement with those of \citet{Giannini04} in terms of pre-shock density, magnetic field, and shock type and age, but our value of the shock velocity is smaller than theirs. Several factors could account for this difference, which might not be a real discrepancy, given the degeneracy of our fitting models. The first factor is that their value lies slightly outside the range of our parameter search. In addition, we studied HH320A\slash B, rather than HH320A. Furthermore, we added the pure rotational transitions of H$_2$ to the analysis. Finally, our shock model incorporates an update of the H--H$_2$ collisional rate coefficients, following \citet{Wrathmall07}.

The parameters of the SiO knot are not as well constrained, as only the pure rotational observations are available to build the H$_2$ excitation diagram. Similarly to the HH objects, the best fitting models are of non-stationary shocks with velocities in the range of 15--35~km~s$^{-1}$ for a pre-shock density of 10$^4$~cm$^{-3}$ (with ages dependent on the value of the magnetic-field parameter). Additionally, a few models with a pre-shock density of 10$^5$~cm$^{-3}$ are found to fit the observations equally satisfactorily, with even more moderate shock velocities (10--20 km~s$^{-1}$) and lower shock ages (which again depend on the value of the magnetic-field parameter). Examples of the comparisons between observations and models are shown in the three upper panels of Figure~\ref{Figure2}, for the cases of the SiO knot, HH320A\slash B and HH321A\slash B, respectively. In each panel, the parameters corresponding to the selected shock model are also indicated.

For the three other points studied(\lq knot 5', \lq knot 6', and \lq knot 8'), once again the excitation diagrams do not constrain the parameters as tightly as in the HH regions, since only the pure rotational transitions of H$_2$ can be used. The number of models that fit these data is large, but we show some examples of the best fits that we could derive in the lower panels of Figure~\ref{Figure2}. We note that the modelling work conducted for these positions also suggests similar excitation conditions, regardless of their association with one lobe of the outflow or the other.

\section{SiO observations and modelling}
\label{sec:SiOoam}

\subsection{Observations}
\label{sub:SiOo}

The observations were carried out mainly in two observational runs, in August and October 2009, with the Atacama Pathfinder EXperiment (APEX\footnote{This publication is partly based on data acquired with the Atacama Pathfinder EXperiment (APEX). APEX is a collaboration between the Max-Planck-Institut f\"ur Radioastronomie, the European Southern Observatory, and the Onsala Space Observatory.}, \citealt{Guesten06}). We used the facility's own APEX--1 and APEX--2 receivers (see respectively \citealt{Vassilev08}, \citealt{Risacher06}) to observe respectively the SiO (5--4) and (6--5) transitions, and the SiO (8--7) transition, in combination with the MPIfR Fast Fourier Transform Spectrometer backend (FFTS, \citealt{Klein06}). Focus was checked at the beginning of each observing session, and after sunrise on Mars. Line pointing was locally checked on 07454--7112 or IRAS 15194--5115. The pointing accuracy was found to be of the order of 5$''$ rms. Table~\ref{table3} contains the main characteristics of the telescope for the observed transitions:~ beam sizes, forward and beam efficiencies, typical system temperatures, and the spectral resolution that was used for each transition. The observations were performed in position-switching mode using the APECS software (\citealt{Muders06}), with a reference position at offset (-600$''$,600$''$) from the central position indicated in Table~\ref{table1}. The data were reduced with the CLASS software (see http://www.iram.fr/IRAMFR/GILDAS).

\begin{table}
\caption{Observed lines, frequencies, and corresponding telescope parameters:~beam and forward efficiencies, beam sizes, typical system temperatures, and spectral resolution.}
\label{table3}
\centering
\begin{tabular}{c  c  c  c }
\hline
line & SiO (5--4) & SiO (6--5) & SiO (8--7) \\
\hline \hline
$\nu$ (GHz) & 217.105 & 260.518 & 347.331 \\
\hline
$B_{\rm eff}$ & 0.75 & 0.75 & 0.73 \\
$F_{ \rm eff}$ & 0.95 & 0.95 & 0.95 \\
\hline
beam ($''$) & 28.7 & 24.0 & 18.0\\
$T_{\rm sys}$ (K) & 155--175 & 270--300 & 275--335 \\
$\Delta$v (km s$^{-1}$) & 2.02 & 1.69 & 1.26 \\
\hline
\end{tabular}
\end{table}

\subsection{Results}
\label{sub:SiOr}

The observations resulted in one SiO (5--4) map of the inner, upper (red) lobe, as well as in SiO (6--5) and (8--7) spectra, obtained by pointing the telescope at designated positions inside this lobe. The absolute coordinates of the (0$''$,0$''$) position are given in Table~\ref{table1}.

\begin{figure}
\centering
\includegraphics[height=9cm,angle=-90]{16758fg3.eps}
\caption{Upper internal part of the BHR71 outflow. The background map is the same as in Figure~\ref{figure1}. The SiO (5--4) contours, which are overlaid in a dark blue colour, correspond to levels of 6 to 30~$\sigma$, in steps of 3~$\sigma$, for an integration between $-$10 and 60 km s$^{-1}$. The half-maximum, 15~$\sigma$ contour is displayed in red. The associated beam size is indicated in the upper left corner. Our SiO (5--4) coverage is actually wider than the field displayed on this Figure.}
\label{figure3}
\end{figure}

The map of the SiO~(5--4) line covers a roughly rectangular region, extending from the lower left offset (35$''$,25$''$) to the upper right (-60$''$,170$''$), and was performed in raster mode, spending 30~seconds on each point. The beam sampling was 10$''$, which is less than the half beam size of 14.35$''$, meaning the map is fully Nyquist sampled. The result is plotted in Figure~\ref{figure3}: the SiO emission, integrated between $-$10 and 60~km~s$^{-1}$, is displayed in dark blue contours overlaid on the H$_2$~0--0~S(5) map already shown in Figure~\ref{figure1}. The half-maximum signal contour is shown in red. The r.m.s. of the SiO~(5--4) map was found to be 0.26 K~km~s$^{-1}$ at the resolution 2.02~km~s$^{-1}$, and the contours correspond to levels of 6 to 30~$\sigma$, in steps of 3~$\sigma$. The contours show that the SiO~(5--4) emission peaks outside of the \textit{Spitzer} spectral line maps, at a position that will be referred to as the \lq SiO peak', with offset (-15$''$, 87$''$). In order to perform a simultaneous study of the H$_2$ and the SiO emission, the point to be studied must be located inside the \textit{Spitzer} map:~we chose the point of maximum emission of H$_2$, at an offset of (0$''$, 77$''$), to which we refer as the \lq SiO knot'. We consider the shift between the APEX SiO~(5--4) and \textit{Spitzer} H$_2$~0--0~S(5) emission peaks to be real, as it is far too large to be attributable to pointing errors. Indeed, the distance between the south-eastern and the north-western tips of the half-maximum SiO emission (roughly of respective coordinates (0$''$,70$''$) and ($-$30$''$,110$''$), see Figure~\ref{figure3}) is about 50$''$, which amounts to 40$''$ once deconvolved from the SiO~(5--4) telescope beam size. Consequently, we consider that, in this direction, which coincides with the line between our SiO knot and peak (see Figure~\ref{figure3}), the emitting region is extended enough to allow us to consider that the signal observed at the position of the SiO knot is free of any residual signal from the SiO peak. Moreover, from the extension of the \textit{Spitzer} maps, it is impossible to exclude the presence of another, potentially stronger peak of H$_2$ emission, coinciding with the SiO peak. In order to check, we overlaid our map on the four (way more extended) channel maps of IRAC, especially the fourth, at 8~microns, whose broadband intensity is dominated by the 0--0~S(4) and S(5) transitions of H$_2$ in this region (\citealt{Neufeld09}). We found that these overlays fail to confirm the existence of an H$_2$ peak coinciding with that of the SiO~(5--4) emission.

\begin{figure}
\centering
\includegraphics[height=9cm,angle=-90]{16758fg4.eps}
\caption{The spectra obtained in the three observed SiO transitions at the positions of the SiO peak and knot, of respective offsets (-~15$''$,87$''$) and (0$''$, 77$''$). Only the SiO knot is considered in our modelling. For each spectrum, we adopted the SiO (5--4) spatial resolution. The ambient cloud velocity, -4.5 km s$^{-1}$ is indicated by the vertical dashed lines.}
\label{figure4}
\end{figure}

The spectra that we obtained of the SiO (5--4) transition at both the SiO peak and knot are presented in Figure~\ref{figure4}, along with the spectra of the other two SiO transitions. In the case of the SiO (5--4) transition, the original beam size was 28.7$''$. In order to derive the spectra at the two selected positions as exactly as possible, we resampled the data with a spatial resolution of 5$''$ and then averaged the four spectra closest to the two positions to obtain the results that are presented on Figure~\ref{figure4}. In the case of the SiO (6--5) and (8--7) transitions, in addition to this spatial resolution problem, we had also to convolve the data to the SiO (5--4) beam size in order to render the whole set of transitions consistent. After this preliminary convolution, we obtained the spectra displayed in Figure~\ref{figure4}. Our mini-maps around the two positions were extended enough to cover the larger beam of the SiO (5--4) observations.

The shape of the line profiles is typical of bipolar outflows (similar, for instance, to those acquired around L1157: see \citealt{Nisini07}), peaking near the cloud velocity and with the main signature being the line wings extending to about 50~km~s$^{-1}$, most visible in the SiO(5--4) line profile of the peak. Such wings seem to be present, though narrower, at higher frequencies. However, it is then more difficult to estimate their width, as the signal-to-noise ratio decreases as the observed frequency increases. The observed SiO probably arises from a complex mixture of shocks with different velocity projections on the line of sight. The velocity range of our shock models does not exceed the terminal velocity of 50~km~s$^{-1}$. On the SiO (5--4) and (6--5) spectra associated to the SiO peak, a velocity bullet seems to arise between 20 and 50~km~s$^{-1}$. It could arise from a process that alters the SiO emission within the region of the shock considered, such as an abundance effect, or from the presence of another shock, with a different velocity, within the telescope beam. These possibilities are discussed in Subsection~\ref{sub:mr} but cannot be thoroughly investigated, given the large beam sizes associated with these transitions; they call for a more detailed study, with higher spatial resolution.

The last step was to derive integrated intensities from these spectra. The results for the SiO knot, which is considered in our subsequent analysis, are shown in Table~\ref{table4}:~integrated intensities and associated r.m.s. are given. The velocity interval over which the integration was made was [$-$10, 60]~km~s$^{-1}$ for all three transitions. Again, the values inferred are consistent with results for other outflows, such as L1448 or L1157 (\citealt{Nisini07}), for which the central source is also a young Class 0 proto-star with a similar bolometric luminosity (respectively, around 13.5, 11, and 1.5--3.5~L$_\odot$ for BHR71, L1157, and L1448; see \citealt{Neufeld09}). In particular, the line profiles we observe for SiO (5--4), (6--5), and SiO(8--7) are remarkably similar to those of L1157-B1, peaking near the cloud velocity. The integrated intensities we inferred are also very close to those compiled for each knot of the L1157 bipolar outflow (\citealt{Nisini07}).

\begin{table}
\caption{Integrated intensities and r.m.s. for the three observed SiO transitions at the position of the SiO knot, of relative coordinates (0$''$, 77$''$).}
\label{table4}
\centering
\begin{tabular}{c c c c}
\hline
line & SiO (5--4) & SiO (6--5) & SiO (8--7) \\
\hline \hline
$\int T_{\rm{MB}} \Delta \varv$ (K km s$^{-1}$) & 7.7 & 4.1 & 1.8 \\
$\sigma_{\int T_{\rm{MB}} \Delta \varv}$ (K km s$^{-1}$) & 0.4 & 0.4 & 0.2 \\
\hline
\end{tabular}
\end{table}

\subsection{Modelling results}
\label{sub:mr}

We derive emission-related quantities by means of a radiative transfer code used in combination with the shock models presented above. The radiative transfer code is based on the LVG approximation, and has been described and used in G08a and G08b. At each point of the shock model, it uses the computed parameters of relevance, such as the temperature, density, velocity gradient, and collision-partner density, to solve the equations of statistical equilibrium and calculate emission-related quantities, such as the level populations, optical depths, and local emissivities. The set of equations is solved by means of a simple lambda-iteration, that stops when the relative difference between each of the level populations computed in two successive iterations drops below a convergence value of 10$^{-4}$.  The set of collisional rate coefficients for SiO with H$_2$ as a collision partner is simply scaled by the square root of the reduced mass ratio from the SiO--He rate coefficients calculated by \citet{Dayou06}. The LVG code also provides the integrated intensity over the whole shock model for all transitions considered.

\begin{figure}
\centering
\includegraphics[width=6cm]{16758fg5.eps}
\caption{Examples of fits of the integrated intensities of our three transitions of SiO. On the $y$-axis is the integrated intensity (K~km~s$^{-1}$), and on the $x$-axis is the rotational quantum number of the upper level of the transition. The observations are the black squares linked by the thick black lines, on all three panels. The 3$\sigma$ errorbars are shown in the Figure. The model results are displayed in colour (blue and red), with the indication of the specific shock parameters on each panel. (a) C-type shock models: best fit shock parameters $n_{\rm H} = 10^4$~cm$^{-3}$, no SiO initially in the grain mantles; (b) CJ-type shock models: best fit shock parameters $n_{\rm H} = 10^4$~cm$^{-3}$ and $\varv_{\rm s} = 28$~km~s$^{-1}$, with 1\% of elemental silicon initially in the grain mantles, as SiO; (c) CJ-type shock models: best fit shock parameters $n_{\rm H} = 10^4$~cm$^{-3}$ and $\varv_{\rm s} = 30$~km~s$^{-1}$, with 10\% of the silicon initially in the grain mantles as SiO.}
\label{figure5}
\end{figure}

The silicon chemistry is extensively discussed in G08a and G08b. Regarding the initial distribution of silicon-bearing material, G08a made the assumption that Si is initially present exclusively in the grain cores, in the form of silicates, with a fractional abundance of $3.35 \times 10^{-5}$ relative to total H. G08b introduced an alternative scenario, in which the Si is partly in the grain mantles, in the form of SiO. Such an assumption was found to be necessary to fit both the SiO and H$_2$ line intensities by means of a single shock wave model. Furthermore, a simultaneous fit can be achieved only by means of a non-stationary, CJ-type shock. When computing CJ-type models in the present study, we adopt one of three values of the fraction of elemental silicon initially in the form of SiO in the grain mantles, namely 0.00, 0.01, or 0.10.

In the first case, when no SiO is initially present in the grain mantles, the gas-phase silicon is produced by the erosion of the grain cores only, which occurs, in the C- and CJ-shock models, where the predominantly charged grains collide with the neutral particles at the ion-neutral drift speed (ambipolar diffusion). Three reaction paths then lead to the formation of SiO in the gas phase, namely Si$^+$(OH,H)SiO$^+$(H$_2$,H)HSiO$^+$(e,H)SiO, Si(OH,H)SiO, and Si(O$_2$,O)SiO; the last two reactions predominate. Following G08a, we adopted the rate coefficient that was experimentally measured for the Si+O$_2$ reaction by \citet{Lepicard01} for both Si+O$_2$ and Si+OH. In the second case, in which SiO is initially present in the grain mantles, their rapid erosion by sputtering in the shock wave generates SiO directly in the gas phase (see also the discussion in G08b).

O$_2$ is a key reaction partner in the process of formation of SiO in the gas phase, and so its abundance must be modelled to the greatest possible accuracy. Furthermore, the question of the pre-shock abundance of O$_2$ in the gas phase must be considered carefully. In all cases, as in G08a and G08b, we used an initial gas-phase abundance of $n(\rm{O_2})/n_{\rm H} = 1.0 \times 10^{-7}$, consistent with the O$_2$ observations of the Odin satellite (see \citealt{Pagani03,Larsson07}). On the other hand, the initial fractional abundance of O$_2$ in chemical equilibrium is $1.0 \times 10^{-5}$; we allocated the difference between these two values (i.e. most of the initial O$_2$) to the grain mantles, consistent with G08a and G08b. Given that the O$_2$ in the mantles is released rapidly into the gas phase, by sputtering processes induced by the shock wave, this scenario does not differ significantly from that in which all of the O$_2$ is assumed to be present initially in the gas phase (the chemical equilibrium situation). An alternative hypothesis, in which the same fraction of the corresponding elemental oxygen is assumed to be in the form of water ice, rather than O$_2$ ice, was considered by G08a and found not to modify significantly the results of the models. Indeed, in this case, the rapid erosion of the grain mantles during the passage of the shock wave releases H$_2$O into the gas phase, and the subsequent reaction of H$_2$O with H produces OH, which then reacts with Si to form SiO. A third scenario was put to the test in the present study: placing the elemental oxygen in the grain mantles in the form of CO$_2$ ice. In this case, CO$_2$ is released quickly into the gas phase during the passage of the shock wave, but no chemical reactions convert it to O$_2$ or OH. When SiO is present in the grain mantles, direct sputtering is the dominant source of the gas-phase SiO. However, when SiO is absent from the grain mantles, erosion of the silicon-bearing grain cores is the mechanism that releases silicon into the gas phase, and the deficit in O$_2$ or OH leads to lower abundances of gas-phase SiO and weaker SiO line emission from low-velocity shocks. In high-velocity shock models, or at higher pre-shock densities, O$_2$ and OH are destroyed in the gas-phase, through the O$_2$(H,O)OH and OH(H,O)H$_2$ sequence, and so the initial composition of the grain mantles is less significant.

If one ignores the observations of H$_2$, it is possible to fit the observations of SiO by means of  C-type shock models, without any SiO initially in the grain mantles; cf. G08a. In this case, we find that shock models with a pre-shock density of 10$^4$~cm$^{-3}$ provide better fits than those with pre-shock densities of 10$^5$ or 10$^6$~cm$^{-3}$. The typical shock velocities are from 25 to 30 km s$^{-1}$, with values of the magnetic-field parameter from 0.45 to 2. An example of such a fit can be seen in panel (a) of Figure~\ref{figure5}. We note that, in this case, the assumption that most of the O$_2$ is initially in the form of CO$_2$ ice on the grain mantles leads to insufficient levels of SiO emission, as compared with the observations. However, our aim is to model simultaneously the emission of SiO \textit{and} H$_2$, assuming their emitting regions coincide, to within the spatial resolution of the observations. Accordingly, we calculate the SiO spectrum for the shock models that already fit the H$_2$ lines, namely the non-stationary shock models presented in Subsection~\ref{sub:cafc}. Given the the additional flexibility afforded to these models by the initial fractional abundance of SiO in the grain mantles, we found that most of the CJ-type models that already fit the H$_2$ data can reproduce the SiO emission satisfactorily. The results are presented in Figure~\ref{figure5}, where panels b) and c) correspond to our best fitting models with, respectively, 1\% and 10\% SiO initially in the mantles. We find that no model in which SiO is absent from the grain mantles is able to reproduce the intensities of the SiO lines simultaneously with those of H$_2$, thereby confirming a conclusion of G08b and rendering considerations of the initial chemical form of oxygen irrelevant.

We wish to emphasize that a single, plane-parallel CJ-type shock wave model is unlikely to provide a completely satisfactory simulation of the molecular line emission from an object as complex as BHR71. In particular, a combination of C-type shock models with appropriate parameters and filling factors might also be able to reproduce the H$_2$ and SiO line intensities and address the problem of fitting the SiO line profiles. The latter could be strongly affected by geometrical effects, associated with the projection of multiple shock velocities on to the line of sight. However, such a study introduces additional free parameters that are insufficiently constrained by the currently available observations. Furthermore, our model does not take into account the consequences of grain-grain collisions, whose inclusion (following \citealt{Guillet07, Guillet09, Guillet11}) would have major implications for computation times. In view of these limitations, geometrical and physical, it is not feasible currently to investigate the nature of the bullet that we observe in the SiO(5--4) line profile.

\section{Water emission predictions}
\label{sec:wep}

\subsection{Water modelling}
\label{sub:wm}

The abundance of water at each step of the calculation is the result mainly of two formation pathways. One is the O(H$_2$,H)OH(H$_2$,H)H$_2$O sequence, which takes place in the gas phase and becomes significant when the temperature exceeds a few hundred kelvin (e.g. \citealt{Charnley97,Atkinson04}). The other is the sputtering of water ice that formed in the mantles from O and H atoms, which were adsorbed on to the grains in the parent dark cloud (see for example \citealt{Tielens82}). In the latter case, the sputtering process is analogous to that considered for SiO when present in the grain mantles.

The modelling of water emission was performed in a similar manner to that of SiO. Again, we used an external radiative transfer module based on the LVG approximation; the molecular data were taken from the LAMDA database (http://www.strw.leidenuniv.nl/$\sim$moldata/). Regarding the rate coefficients for excitation of H$_2$O by He, we used the data of \citet{Green93}. For collisions of H$_2$O with H$_2$, we adopted the same approach as FP10 and used the CTMC results of \citet{Faure07}, rather than the more precise but less complete (in terms of their temperature range) quantal calculations of  \citet{Dubernet02}, \citet{Grosjean03}, and \citet{Dubernet09}. As no data exist for the excitation of H$_2$O in collisions with H, we used the same rate coefficients as for excitation by ortho-H$_2$, following FP10.

The more complex structure of H$_2$O, as compared to SiO, results in some changes being required to the computational method in the radiative transfer module. First, the code must be  modified to take account of the more complicated radiative selection rules. Second, in the more complex case of water as compared to SiO, a value of 10$^{-10}$ is required for the convergence parameter. Finally, we found it necessary to adapt the expression that is used for the escape probability. For a plane-parallel geometry, such as is assumed in our shock models, the escape probability is

\begin{equation}
\label{eq:betaiso}
\beta_\perp = \frac{1 - e^{-\tau_\perp}}{\tau_\perp}.
\end{equation}
where $\tau_\perp$ is the LVG optical depth in the $z$-direction, normal to the shock front. On the other hand, \citet{Neufeld93} proposed the following approximation to the angle-averaged escape probability,
\begin{equation}
\label{eq:betaplane}
\bar\beta_{\rm av} = \frac{1}{1 + 3\tau_\perp},
\end{equation}
In the case of water, we found that the use of the second formula gave rise to numerical instabilities and longer computation times. Consequently, we adopted the first formula, both when solving the equations of statistical equilibrium and when evaluating the local line emissivity at each point in the shock wave. This approach is consistent with that of FP10 and enables us to make direct comparisons with results obtained using their method of treating radiative line transfer in shock waves. The implications of the different forms of the escape probability for the intensities of the rotational transitions of SiO are discussed in Appendix~A of G08a. We recall that the geometry of the shock wave is not well known.

Before comparing with the method of FP10, we benchmarked our LVG code against the RADEX code (\citealt{Vandertak07}), at four representative points, covering different conditions of temperature, density, and velocity gradient, namely (respectively in K, cm$^{-3}$, and s$^{-1}$): ($25$, $10^4$, $2\times10^{-13}$), ($50$, $10^5$, $10^{-13}$), ($300$, $10^4$, $10^{-12}$), and ($467$, $3.71\times10^5$, $9\times10^{-11}$). For the purpose of this comparison, we adopted the same escape probability formula as in the RADEX code. For ortho-H$_2$O, the computed excitation temperatures showed no mean relative discrepancy above 6.3\% for the ten levels emitting the strongest lines at each of the four points. In the case of para-H$_2$O, the relative discrepancy was occasionally larger, reaching 43.9\%. Although it remains unclear why the discrepancies were larger for para- than for ortho-H$_2$O, the overall level of agreement with the RADEX code was reassuring.

\subsection{Steady-state versus statistical-equilibrium}
\label{sub:ssse}

      \begin{figure*}
   \centering
   \includegraphics{16758fg6.eps}
      \caption{Upper panels:~comparison between profiles obtained when the computation of the water line emission is internal to the shock code (steady-state approximation: blue curves) or external to the shock code (statistical equilibrium approximation: red curves);~the temperature of the neutral fluid (continuous line) and the fractional abundance of water (dashed lines) are shown for our two reference, C-type (left-hand panel), and CJ-type (right-hand panel) shock models. In both cases, the shock parameters are displayed in the corresponding panels. Lower panels:~integrated line intensities for all para-water transitions;~steady-state approximation to the computation of the water emission (dark blue open circles); same shock model, but with the statistical-equilibrium approximation to the computation of the water emission (large light-blue open circles); present shock model, with the statistical-equilibrium assumption (small red filled circles).}
         \label{Figure6}
   \end{figure*}

       \begin{figure*}
   \centering
   \includegraphics{16758fg7.eps}
      \caption{Evolution of the computed local optical depths of two transitions as a function of the flow time of the neutral fluid in our reference models, the stationary C-type (left panel) and non-stationary CJ-type (right panel). The o-H$_2$O 1$_{\rm{10}}$--1$_{\rm{01}}$ (at 557~GHz) and p-H$_2$O 1$_{\rm{11}}$--0$_{\rm{00}}$ (at 1113~GHz) lines are considered, and their optical depths are shown in blue and red, respectively. The corresponding total optical depths are indicated in the same colour code.  The neutral temperature profile shown in black. The shock parameters are specified in each panel.}
         \label{Figure7}
   \end{figure*}

In this section, we compare the results of the present calculations with those obtained using the approach of FP10. We present the intensities of all ortho- and para-transitions, integrated over the whole extent of the shock wave. We compared one stationary C-shock model, with input parameters $n_{\rm H}~=~2\times$10$^4$~cm$^{-3}$, $\varv_{\rm s}~=~20$~km~s$^{-1}$, and b = 1, and one non-stationary CJ-shock model, with input parameters $n_{\rm H}~=$~10$^4$~cm$^{-3}$, $\varv_{\rm s}~=~28$~km~s$^{-1}$, b = 1.5, and age 500~yrs, which fits both the H$_2$ and SiO observations (see Figure~\ref{figure5}, panel b). The principal difference between the two versions of the shock code is that FP10 included the population densities of the levels of water as variables of the model, and the differential equations describing the evolution of the level populations were solved simultaneously with those for the other dynamical and chemical variables, in the steady-state approximation. Thus, the water line emissivities were computed within the shock code, at each point of the shock profile, and could be integrated internally. In the present approach, the level population densities (in statistical-equilibrium) and the line intensities are calculated in a separate LVG module, to which the shock profiles are provided as input data.

In addition to the different approximations used when calculating the population densities of the water levels (steady-state\footnote {$\partial/\partial \it{t}$ = 0 and hence $\rm{d} / \rm{d} \it{t} = \it{\varv} \rm{d} / \rm{d} \it{z}$} and statistical-equilibrium\footnote{$\rm{d} / \rm{d} \it{t} \equiv 0$}), there are two further, potentially significant differences between these two sets of calculations. In the steady-state case, the radiative cooling function that is calculated at each point includes the contribution of the water emission, determined from the level population densities and the line escape probabilities. This contribution has an effect on the temperature profile in regions where H$_2$O is a significant coolant. In the statistical-equilibirum assumption, the contribution of water emission to the cooling of the medium is approximated by means of the tables provided by \citet{Neufeld93}. In addition, the effect of adsorption of gas-phase species on the radius of the grains is treated differently in the two versions of the shock code; this affects the gas--grain interactions in the tail of the cooling flow, where adsorption takes place. As a consequence, the coupling of the gas to the grain temperature, as the post-shock region is approached, occurs differently in the two versions of the shock code.

In both the C-type and CJ-type cases, we have three sets of LVG calculations. We denote by `FP10'  the results of the steady-state (s-s) shock code. Additionally, the dynamical and chemical profiles generated by either version of the shock code may be combined with a separate,  statistical-equilibrium (s-e) treatment of the water level populations. The upper panels of Figure~\ref{Figure6} compares the neutral temperature and water fractional abundance profiles from the two versions of the shock code. In the case of the C-type model, differences are noticeable only in the cooling flow, where water is a significant coolant (see top right panel of Figure~2). Nonetheless, the differences in the thermal profiles are modest, and the water fractional abundances in the two versions remain indistinguishable. In the case of the CJ-type model, even a small displacement of the location of the J-discontinuity can modify the maximum neutral temperature, which in turn has an effect on the fractional abundance profiles: see the r.h.s. upper panel of Figure~\ref{Figure6}.

The lower panels of Figure~\ref{Figure6} show the integrated intensities of the total of 156 transitions of para-H$_2$O that result from the three different calculations. In the case of the C-shock, the similarity of the results is striking and extends to very weak lines. The time-scale for the level populations to approach equilibrium is given by $[n(\rm H_2)\it q(J+1 \rightarrow J)]^{\rm{-1}}$ (where $q(J+1 \rightarrow J)$ is the de-excitation rate coefficient for collisions with molecular H$_2$) in the limit of high densities; it is even shorter in the limit of low densities, when radiative decay dominates collisional de-excitation. To validate the assumption of s-e, one must compare this population transfer time-scale with a dynamical time-scale, such as the flow time of the neutral particles through the shock region, that corresponds to the width of the neutral temperature profile shown in the upper panels. Adopting the representative values of 10$^4$~cm$^{-3}$ for the density and 10$^{-10}$~cm$^{-3}$ for the collisional de-excitation rate coefficient results in a population transfer time-scale of 0.03~yr, much less than the flow time of the neutral particles through the C-type shock considered. In the case of the reference CJ-type shock model, this condition is verified for most of the transitions, as the overall agreement between light and dark blue open circles in Figure~\ref{Figure6} confirms. For the brightest transitions, our independent LVG calculation is consistent with that denoted `FP10'. In this case, the discrepancies with the red filled circles are larger, owing to the differences in the water abundance profiles, which are attributable in turn to the temperature differences arising from: the small displacement of J-discontinuity; the treatment of the cooling due to water; and the strength of the grain--gas interaction as the post-shock region is approached. We note that the pattern created by each set of points is similar for the brightest, and hence observable, transitions, and that the pattern is shifted vertically from one set of results to the other. Such a shift is indistinguishable from that arising from the uncertainty in the filling factor, when comparisons are made with observations.

We conclude from the above analysis that the use of the s-e approximation is justified in the present context of the study of water emission.

\subsection{Water emission predictions for BHR71}
\label{sub:wepfBHR71}

As a preamble to this section -- aimed at providing predictions of water line intensities for use in the interpretation of observations -- we study the evolution of the optical depth of the fundamental transitions of both o-H$_2$O and p-H$_2$O in each of our reference models. This evolution, together with the total optical depths, integrated through the shock wave, are shown in Figure~\ref{Figure7}. Owing to the one-dimensional nature of our approach, we probably overestimate the optical depths and find that the transitions are optically thick in most parts of our shock models; this is especially the case of the C-type shock, as the water accumulates in the large post-shock region. The example of the CJ-type shock shows the spread of values of the optical depths in the emitting region -- low when water is dissociated in the high-temperature regime, followed by higher values when water reforms. This figure underlines the requirement for an adequate treatment of the radiative transfer.

As already mentioned, H$_2$, SiO and H$_2$O are believed to have coincident regions of emission, at least to the resolution of currently available observations (e.g. \citealt{Nisini10}). For completeness, we provide predictions of water line intensities for \textit{all} the models that were found to fit the H$_2$ pure rotational excitation diagram acceptably at position of the SiO knot. Given the relative uniformity of the shock conditions in the inner parts of the outflow, revealed by the similarity of the H$_2$ excitation diagrams at the different positions considered, our models should be applicable to water observations at any position. Stationary, C-type shock models are excluded, for the reasons given in Section~\ref{sub:mr}.

The results are given in Tables~\ref{tableb1} and \ref{tableb2} for o-H$_2$O and p-H$_2$O, respectively. The transitions that appear in the Tables are the ones that will be the target of \textit{Herschel} observations. The first three transitions in each table will be observed by HIFI, and the remainder (nine transitions of o-H$_2$O and three of p-H$_2$O) will be observed by PACS, in the framework of the WISH key-program (\citealt{Vandishoeck11}). The calculations comprise the entire set of transitions that are listed on the LAMDA website, and the complete results are available upon request.

The first general comment concerns the dependence of the water emission line intensities on the pre-shock density. We find that the integrated intensities calculated for a pre-shock density of 10$^5$~cm$^{-3}$ are systematically around one order of magnitude larger than those computed in models with pre-shock densities of 10$^4$~cm$^{-3}$, regardless of the values of the other parameters, such as the shock velocity or magnetic-field strength. In addition, and with all other parameters remaining equal, we find that the computed integrated intensities vary by factors of 2--3, and sometimes more, over the range of shock ages considered; this variation may be sufficient, in certain circumstances, to enable the observations to constrain the age of the shock wave.

Finally, we consider the computed data pertaining to the eight shock models that provide the best simultaneous fits for H$_2$ and SiO; these models are shown in Figure~\ref{figure5}, in panels (b) and (c). The results of the calculations of the integrated intensities of the brightest o- and p-H$_2$O transitions, likely to be targetted by HIFI and PACS, are shown in Figure~\ref{figure8}. The filling factor is assumed to be the same and equal to 1 for all the transitions and too small to discriminate between these models. Nevertheless, forthcoming \textit{Herschel} observations should enable us to enhance our understanding of the chemistry of water in interstellar shock waves.

Water is believed to be the main interstellar reservoir of oxygen, which is the most abundant element in the universe after H and He and plays a major role in interstellar chemistry. Given its rotational energy level structure, water is an important gas coolant and a convenient tracer of shocked regions. Forthcoming observations, through their comparison with the predictions of shock models, should enable us to investigate both the chemical and the physical processes at work in bipolar outflows.

   \begin{figure}
   \centering
   \includegraphics[width=9cm]{16758fg8.eps}
      \caption{Integrated intensities of the strongest transitions of o- and p-H$_2$O to be targeted by HIFI and PACS, for the eight shock models presented in panels (b) and (c) of Figure~\ref{figure5}. The o-H$_2$O and p-H$_2$O transitions are indicated by circles and squares, respectively. The shock model parameters are abbreviated such that  \lq n4b1.50v28t500', for example, corresponds to a pre-shock density of 10$^4$~cm$^{-3}$, a magnetic-field parameter of 1.5, a shock velocity of 28 km s$^{-1}$, and an age of 500 years.}
         \label{figure8}
   \end{figure}

\section{Concluding remarks}
\label{sec:cr}

We have presented a detailed analysis of observations at a few positions in the the bipolar outflow BHR71, assuming that the emission from these regions arises in shock waves. In two cases, namely the Herbig-Haro objects HH320 and HH321, we are able to make use of both the recent \textit{Spitzer} observations of pure rotational transitions and previous, ground-based observations of rovibrational transitions of molecular hydrogen. In order to compare with the predictions of our shock models, we used excitation diagrams. The physical conditions were found to be similar in both cases, with a pre-shock density of 10$^{4}$~cm$^{-3}$ and moderate shock velocities, in the range 15--35~km~s$^{-1}$. The only shock models that fit these data satisfactorily are non-stationary, with ages that depend on the magnetic-field strength and do not exceed 2000~years. Three other positions in the upper and lower lobes of the outflow were studied, using only the pure rotational transitions of H$_2$ observed by \textit{Spitzer}. Our analysis suggests that the excitation conditions at these positions are similar to those in the HH objects and can only be reproduced by non-stationary models.

We present a new map of the SiO(5--4) transition in the inner part of the bipolar outflow BHR71, together with new observations of the SiO(6--5) and SiO(8--7) lines, at one position that is also covered by the \textit{Spitzer} observations and at another position that lies outside of the \textit{Spitzer} maps. At the first position, referred to as \lq the SiO knot', we make use of the combination of data (pure rotational transitions of both H$_2$ and SiO) in order to constrain the parameters of our shock models more tightly than is possible with the rotational transitions of H$_2$ alone. The modelling based on H$_2$ leads to the conclusion as for the other positions in the outflow, namely non-stationary shocks provide the best fits. In particular, shocks with a pre-shock density of 10$^{5}$~cm$^{-3}$, low velocities (10--20~km~s$^{-1}$) and ages (less than 1000~years) were found to be good candidates. Including the SiO emission places constraints on the initial repartition of silicon-bearing material but is of little help in discriminating between the models which fit the H$_2$ rotational excitation diagram.

We have validated our approach to calculating the water line intensities, which uses the results of shock model as input to a separate radiative transfer code, based on the LVG approximation. To this end, we provide a full comparison between the statistical-equilibrium and the steady-state approximations, based on reference shock models of the stationary, C-type, and non-stationary, CJ-type. We make predictions of water emission line intensities for the SiO knot in the BHR71 outflow. As we expect emission by water to coincide with that by SiO and H$_2$, we provide the results of the LVG calculations of the water line intensities for models that fit satisfactorily both the SiO and H$_2$ emission.\footnote {On request, we can provide water line intensities for all the shock models that fit the H$_2$ observations.} Given that the excitation conditions are relatively uniform in the internal parts of the outflow, we consider that our calculations can be used to compare with observations of water throughout this region.

We shall discuss in a future publication ground-based observations of CO transitions, undertaken with the APEX facility, that could bring further insights into the physical conditions in the BHR71 outflow. Complementary observations of sulphur-bearing molecules and other shock tracers, such as HNCO, are planned. One of the aims of these studies is to investigate the suitability of \lq chemically active outflows', such as BHR71, for observations with the new generation of instruments, such as ALMA.

\begin{acknowledgements}
      BP acknowledges the support of the Deutsche Forschungsgemeinschaft through the Emmy Noether grant PA1692/1--1. We also wish to thank Malcolm Walmsley and an anonymous referee for useful comments that contributed to improving the completeness and clarity of our paper.
\end{acknowledgements}

\bibliographystyle{aa}

redpajama_set_name: RedPajamaArXiv


text:
Franz Karl Stark (3. dubna 1873 Loket – 14. říjen 1952 Neustadt an der Aisch) byl československý politik německé národnosti. Byl meziválečným senátorem Národního shromáždění za Německou sociálně demokratickou stranu dělnickou v ČSR.

Biografie
V parlamentních volbách v roce 1920 získal za Německou sociálně demokratickou stranu dělnickou v ČSR (DSAP) senátorské křeslo v Národním shromáždění. Mandát obhájil v parlamentních volbách v roce 1925 a parlamentních volbách v roce 1929. V senátu zasedal do roku 1935.

Profesí byl sekretářem strany ve Stříbře.

Odkazy

Reference

Externí odkazy
 Franz Karl Stark v Národním shromáždění roku 1920

Senátoři československého Národního shromáždění
Českoslovenští politici německé národnosti
Členové Německé sociálně demokratické strany dělnické v ČSR
Narození v roce 1873
Úmrtí v roce 1952
Narození 3. dubna
Úmrtí 14. října
Muži

redpajama_set_name: RedPajamaWikipedia


text:
La Paloma ist das 18. Extended-Play-Album des österreichischen Schlagersängers Freddy Quinn, das 1961 im Musiklabel Polydor (Nummer 21 906 EPH) erschien und spanische Titel beinhaltete. Alle vier Titel wurden von Quinn auf anderen Tonträgern auch auf Deutsch gesungen. Herstellung und Vertrieb erfolge durch Fonogram S.A. sowie der Druck durch ALG – Madrid.

Plattencover

Auf dem Plattencover ist Freddy Quinn auf Fischernetzen sitzend zu sehen, die sich auf einem Schiff befinden. Er trägt ein Hemd und eine Hose in der gleichen Farbe sowie Stiefel.  Das Plattencover des Vorgängeralbums J'ai besoin de ton amour ist ähnlich gestaltet, dort ist nur das Meer als Hintergrund zu sehen. Bei La Paloma hingegen sind größere Teile des Schiffs, unter anderem ein Rettungsring und ein Schiffsmast ersichtlich.

Musik
La Paloma () ist eine Habanera, die vom spanisch-baskischen Komponisten Sebastián de Yradier (1809–1865) komponiert und um 1863 erstmals gesungen wurde. Das Arrangement stammt von Franz Josef Breuer. Die deutsche Version war eine von Quinns Millionenhits.

Sólo El Viento ist eine spanische Übersetzung von Quinns Lied Nur der Wind, das von Lotar Olias, Aldo von Pinelli und Günter Loose geschrieben wurde.

¿Qué Hacemos Con El Marinero? ist eine spanische Übersetzung des Shantys Drunken Sailor – dessen Melodie wiederum wurde dem Protestlied Oró Sé do Bheatha 'Bhaile entnommen. Auch diese Fassung wurde von Franz Josef Breuer arrangiert.

Nubes, Viento y Velas Blancas ist die spanische Fassung von Wolken, Wind Und Wogen von Lotar Olias und Walter Rothenburg, das Quinn auf seinem Studioalbum Freddy auf großer Fahrt veröffentlichte.

Titelliste

Das Album beinhaltet folgende vier Titel:

 Seite 1

 La Paloma
 Sólo El Viento

 Seite 2

 ¿Qué Hacemos Con El Marinero?
 Nubes, Viento y Velas Blancas

Weblinks

Freddy-Quinn-Album
Extended Play
Album 1961
Album (Schlager)


The Knitting Pirate » In Which the Pirate Swears She's Done Now.
« In Which the Pirate is Frustrated.
In Which the Pirate Swears She's Done Now.
Pirate-Husband laughed at me when I said "After this, I'm not going to buy any more yarn until MD Sheep and Wool in May." Can I really go nine months without buying any yarn? We shall see - but that's my plan!
But this was a special case (aren't they all?) This is Opal Rainforest yarn in the discontinued and hard-to-find Tiger colorway, and I've been looking for two skeins of it for over a year so that I can make matching tiger paw socks for both of us. I finally found some through an Australian Raveler who was kind enough to ship overseas for me!
My favorite animal is the mountain lion, but Pirate-Husband likes tigers better, and so I thought it would be perfect to make him socks like these. Here is a link to the original project on Ravelry. I think they're adorable!
I did tell Pirate-Husband that I have no idea when I'm going to actually get to knit these. But at least now I have the yarn, right?
This entry was posted on Sunday, September 6th, 2009 at 15:51 and is filed under stash, yarn. You can follow any responses to this entry through the RSS 2.0 feed. Both comments and pings are currently closed.
Also you sold that green stuff, doesn't that mean you can buy yarn now?


text:
Gensler selected for new UW college basketball training facility in Seattle
By Josh Niland
Nov 18, '21 11:53 AM EST
Image courtesy Gensler
An ambitious new athletic facility for the University of Washington's men's and women's basketball programs has got the ball rolling thanks to a design from Gensler.
The newly-approved Basketball Training & Operations Facility and Health & High Performance Center is seen as an enhancement of student-athlete life as well as a potential recruiting tool, for a program that has recently missed its shot to attract and retain several high-level future pros.
The project is being paid for entirely through private donations to UW's athletics program, a fact that is especially welcome at a time when the university's funds are in much greater need in other areas of campus life.
The facility will be installed on the current site of the historic Hec Edmundson Pavilion, one of America's oldest college gyms, and will include state-of-the-art new practice courts, locker rooms, dedicated film study rooms, player lounges, and something called an "enhanced performance center."
In related Gensler Sports news: The LA Chargers have tapped Gensler for a proposed new $100 million training facility
The project's architects see it as a metaphor for peer-based collaboration and the spirit of athletic competition.
"Working with the University and Gensler in this integrated approach embodies the spirit of collegiate athletics, where groups of talented individuals of diverse backgrounds and skillsets come together to push the limits of what is possible," said Tamara Hartner, the design phase executive at Gensler's teammate Mortenson.
Approval has already been granted for the facility by the university's board of regents. The project is set to tip off in 2024.
Plans for LA Clippers arena in Inglewood move ahead
AECOM's basketball net-inspired designs for a new Los Angeles Clippers arena are unveiled
Nike transforms historic Chicago church into basketball court for young hoopers
3XN to design new arena in the heart of richly historic Bergen, Norway
10 spectacular performance spaces for your Friday inspiration
John King reviews the new Golden State Warriors arena in San Francisco
basketballuniversity of washingtonseattlesportsarenagensler
Related Archinect Profiles

redpajama_set_name: RedPajamaCommonCrawl


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Restoration, sales, and advice to all string players in the North East and across the UK
Clients Now
Repairs & Restorations
Instrument sales
Buying an instrument
Selling your instrument
Huge thanks to all players who have visited this year. Its been a pleasure to chat/share/resolve issues. Hope your stocking, like mine, is full of joy and really look forward to seeing you in 2022!
December 2021: Many Christmas musical events are happening but if any are cancelled and you are left feeling cheated, please take it from me………inspirational stuff is happening in Cambridge and every year they really do lift my spirits. So, if you have time or the inclination, please do check out King's College website for their festive programme.
I have had the pleasure of being present at Kings College Chapel for many musical events. Of course, one of the most famous, with people travelling from all around the world to witness, being 'Carols from King's'. Tickets sold out weeks ago but we can still be a part of it by simply viewing or listening in our homes. On their website they say…
A Festival of Nine Lessons and Carols is broadcast on BBC Radio 4 and the BBC World Service on 24 December at 3pm (10:00 EST or 07:00 PST). The service is also broadcast at 1pm on Radio 3 on Christmas Day, and at various times on the BBC World Service.
Carols from King's is shown on BBC Two on Christmas Eve (please check the BBC TV guide for the time). This is recorded by the BBC early in December and is a different service from A Festival of Nine Lessons and Carols.
The new year also has a treat for us. I tend to be glued to the Vienna Philharmonic concert on New Year's Day. It's become a tradition. Strauss is in my house all morning! On BBC 2 from 10.30am.
The Vienna New Year's Concert (Neujahrskonzert der Wiener Philharmoniker) is an annual concert of classical music performed by the Vienna Philharmonic traditionally on the morning of New Year's Day in Vienna, Austria.
The 2022 Vienna Philharmonic New Year's Concert will be under the baton of Daniel Barenboim in the Golden Hall of the Musikverein in Vienna. Daniel Barenboim's close musical partnership with the Vienna Philharmonic started in 1965. After 2009 and 2014 the concert on January 1st marks the 3rd time, that Daniel Barenboim conducts this prestigious concert event.
The 2022 New Year's Concert will be broadcast in over 90 countries and followed by millions of television viewers around the world.
Here's to a brighter future where 2022 will allow us to play, enjoy and celebrate our instruments and our music. Cheers!!
judith@judithblackwellviolins.com
Telephone. 01289 304383
Sign up to my newsletter here.
Incredibly sensitive to my needs.
"Judith did an exceptional job on my 1888 Collin-Mezin cello. I can't remember it ever sounding as good as it did after her restoration! Judith was a delight to work with. She listened compassionately to my concerns with the instrument and was incredibly sensitive to my needs. I was delighted that she finished the work two weeks ahead of schedule, which enabled me to use my cello for international performances. I would highly recommend Judith- she is a restorer of the highest quality and I feel so grateful that she was able to work on my instrument."
Just days after collecting Katie messaged……"I just wanted to let you know the cello is sounding absolutely incredible! And everyone is commenting on it! I did a session online a few days ago and my colleague could not believe how resonant the cello sound was. I am so over the moon happy!!"
Katie Tertell
Professional Cellist
Still can't get over this violin!
I'm still completely shocked at its beautiful tone now, and it feels so lovely to play. Never in a million years did I think it would ever sound like it does now – I liked it before, but now….I just have no words. I just wish I'd known you years ago!
Katherine Baxter
I couldn't be happier with the work Judith has done on both instruments.
"I couldn't be happier with the work Judith has done on both instruments. One of them was made by my Great Great Grandfather, and my 10 year old daughter is about to start learning on it. It had always had what I now know to be cigarette burns on it, and they're now gone – I didn't even know getting rid of them was possible! It had quite a bit of other work done, and Judith also provided a new bow and shoulder rest. It's lovely to have it back in working order.
The other one, I have used for the past 30 years, and I had absolutely no idea that it could sound like it now does – it sounds absolutely amazing, and has a much more powerful and warm sound than ever before."
Instantly noticed problems … and suggested what should be done
"She repaired a full size violin and a ⅛ cello for me which had travelled from Tokyo to Berwick. The violin is old and had been repaired many times, including in Japan. She instantly noticed problems and after a careful consultation she suggested what should be done. When the violin was repaired it sounded amazingly good. The ⅛ cello was not severely damaged but needed to be repaired a little and it was really nicely done."
Kuniko Tuda
Really went out of her way to help us
"We are very grateful to Judith both for finding for us the perfect instrument for our daughter and for helping to improve my son's violin. She had listened so carefully to what we were trying to achieve and really went out of her way to help us and to fit in some very subtle but hugely effective adjustments to my son's instrument. Although we live a long way from Judith, we will certainly return to her to help us with some further work to touch up other areas of the varnish on my son's violin. BRAVO!"
Jane Finlayson-Brown
I will always be grateful for Judith's care and attention
"A wonderful job, sensitively returning the cello to its former glory despite the damage being worse than originally imagined. She then provided valuable advice for its insurance and after care. I will always be grateful for Judith's care and attention in returning my precious cello to me."
Sian Scaife
Cellist, Newcastle upon Tyne
Huge bonus to know that my violin will remain in first class condition
"Judith Blackwell has restored my violin to perfection. Judith provided expert advice and guidance for set-up and string choice and I am delighted with the transformative results. It is a huge bonus to know that my violin will remain in first class condition through regular visits to such a distinguished and sympathetic Luthier."
Helen Mason
Violinist, Kensington, London
Feel very lucky to have someone of Judith's skill and expertise
"Judith repaired my grandfather's violin which dates from the end of the 19th century … quite an emotional moment when we saw it again as we could hardly believe how good it looked and sounded. We feel very lucky to have someone of Judith's skill and expertise repair what is, once again, a treasured family heirloom."
Nan MacFarlane
journalist and violinist, Scottish Borders
Judith provides a unique service tailored to the individual
"Judith provides a unique service tailored to the individual customers' requirements, regardless of whether you're a student or a professional. I have known Judith for a long time and I know that whenever I have the smallest problem, she will always be on the end of the phone or make time to see me no matter how busy she is. This commitment and flexibility towards her customers has been critical for me as a player, I often have only small windows of time that I can be without my violin, and Judith will always accommodate this."
Ross Hume
Guildhall Conservatoire, London
Work is of the highest quality
"I am now a retired professional violinist living in Northumberland after spending almost 30 years as a member of the Royal Opera House Orchestra, Covent Garden, London and other major Symphony Orchestras. My violin is very special to me. I am more than delighted with the excellent work carried out by Judith. A problem I had for so long was addressed very quickly, and the work done is of the highest quality. I do not hesitate in recommending any work carried out by Judith."
Retired Professional Violinist, London & Northumberland
© Judith Blackwell 2021


Events, facts, documents and evidences: It has earlier been described in detail on the page "Pollution of Belovezhskaya Pushcha: dumping rubbish and sawdust" about a new polygon or, to be exact, a dumping ground for storage of sawdust and wastes of wood processing which was built in 2004. It is located close to the village of Selishche which is tree kilometer from the village of Kamenyuki (the administrative center of the national park) and a thriving sawmill. Sawdust and other wood processing wastes which were earlier burnt at the central dumping ground near the sawmill are delivered to this ground over the last years. New technologies for manufacture of fuel briquettes or other useful production from sawdust have not been introduced in the national park. Some parts of sawdust are taken by the local population for in-house needs, while the others lay and decay on the dumping ground.
The photos below show how the situation on the dumping ground later developed.
This is the view of the dumping ground on the side close to a road in 2005. The ground covers the area of several hectares and is isolated with a capital fence of height about 2 meters.
A beautiful shield of dark blue colour has been set up on the fence at the both ends of the dumping ground on its side close to the road. The shield has a record "Polygon for storage of organic fertilizers". There are no yet reliable information about that is actually true.
This is the view inside the dumping ground in 2005, that is one year later since the functioning ground.
This is the view inside the dumping ground in 2006, that is two years later since the functioning ground. Sawdust and bark evenly spread upon the area of the dumping ground have been moved by bulldozer to make big and high heaps.
Photos below show the dumping ground in 2008, that is three years later since the functioning ground.
The well-made fence began to collapse as early as 4 years since its construction - wooden poles has got rotten in some places and the fence has tilted and has even fallen here and there. Thus, additional financial resources are already necessary for its repair and restoration.


Cyclone is a dragon shout added by the Dragonborn expansion. When used, the shout fires out a small cyclone that throws enemies, even large enemies like giants, into the air causing moderate damage. The more powerful the shout, the more damage the cyclone does and the farther range it has.
Even a single word of Cyclone can turn the tide of a battle, as it takes enemies a couple of seconds to get up from the ground after being thrown, similar to a one second Paralysis effect.
This page was last modified on 16 April 2019, at 15:58.


This custom built furniture hutch included 8 full extension drawers with soft close hinges , custom countertops and furniture base finish. It integrates nicely with the wrap-around crown moulding and furniture base floor baseboards. The hardware handles for this units are oval chrome pulls.


Three series of BFS critical experiments loaded approximately with 10 kg of 237Np-dioxide were analyzed to verify the performance of major libraries with the 237Np nuclear data. The latest JENDL-3.3, ENDF/B-VII.0 and JEFF-3.1 showed satisfactory results from the 237Np data viewpoint; however some other major data such as 239Pu ν and fission, 238U µ and/or the sodium inelastic scattering cross sections of some libraries may need re-evaluation. Further, the effect of integral experimental information to obtain better predictions of reactor core parameters was demonstrated by the cross section adjustment method.


text:
House L - 2004
2004, Kortrijk (BE)
It was the objective to respect the Neo-Tudor style in its individual character. A passage in glass and a garden wall reconciles itself with the North side of the English country house. Architecture is at stand of man and art. The house gets a new approach, a new perception and the game of reflection and perspective contributes to the propitiation of old and new. In the entrance hall the glass construction ensures transparency in the house, but it is even a threshold to the private part.
The glass passage reaches new possibilities and this architecture offers them an answer on the question to privacy, art and time. The glass is not only a transparent separation, but it is constructively applied as a support of the roof. The minimum cross-section of the glass and the details result in a light architecture that is in contrast to the monolithic English style. This glass passage accompanies us to the pavilion and with a twist we are leaving the house. We reach a place, stipulated by four bluestone pillars and enclosed by glass. This space behaves itself as a peninsula within the design. On this spot interior and exterior amalgamate.
In the cottage excisions are made by slicing and cutting out. Architecture is stripped of architecture. These vacua intensify what is built and are significative. Architecture which exists in what it omits.
Photos by Kristien Daem and Åke E:son Lindman


Peace on Earth Good will to all.
A peace loving Humanist I extend a hand to those of my cultural roots the Xians. I love the identity part of the culture.
Xmas means family reunion & Carols. I love to sing Carols.


Read the article on Information Week web site ..
The European particle physics laboratory CERN used it to detect the elusive Higgs Boson. Wall Street has used it for years to evaluate oceans of market data in order to make high-frequency trades. And the National Security Agency (NSA), we've recently learned, uses it to pore over billions of our emails and text messages….


Gorgeous locations surround you – Laguna Bay and the Coral Sea that lap Noosa's beaches, the winding Noosa River fed by the Everglades, back-to-back national parks and hinterland trails that carry you on foot, bike or horseback.
Stay in absolute beachfront apartments, lakeside cottages, river rooms, hinterland cabins, on a houseboat or glamp under Noosa's starry skies.
There's always something new to discover in Noosa so book your next escape at visitnoosa.com.au or call 1 3000 NOOSA.
Get your wanderlust going and follow @visitnoosa on Instagram and Facebook.
From saltwater to freshwater and green spaces in between, Noosa's nature inspires, restores, soothes and energises you – and provides endless beautiful photo opportunities. The easy access to surrounding national parks, adjoining UNESCO Biosphere Reserves, World Heritage-listed Fraser Island, one of only two Everglades systems in the world, pristine Noosa River and green hinterland offers so many ways to explore some of nature's best.
Immerse yourself in nature on walking tracks with stunning sea views, from on-board relaxing river boats; underwater as you snorkel or dive with marine life; from above on a scenic flight or as you skydive from a plane; on horseback along a beach, across a lake or through forest trails; on a surfboard for the first time; from atop a mountain lookout or as you laze on the beach, only metres from your accommodation.
Swim, sip, savour, surf and swing your way through Noosa and time your holiday to coincide with one of these events that showcase the Noosa lifestyle to a tee!
Join Olympian Michael Klim for a weekend of sun, surf and ocean swims in Noosa's calm, sheltered waters that hug Noosa National Park.
The world's biggest surfing festival is 8 days of pure stoke with events for grommets to grandpas, dogs, body surfers, specialty and pro divisions – and the best beach bar around!
Discover new flavours and great Australian wines with some of Australia's best chefs in beautiful beach, river and hinterland locations.
Swim Noosa, run Noosa and cycle Noosa against the backdrop of Noosa's beautiful beach, river and hinterland.
Just relax, they say … when it's time to step out of your busy life, step right into relaxation, pampering and calm as Noosa's natural beauty inspires you to focus on health and well-being, even when on holiday.
Start with a sunrise jog on the beach or stroll through Noosa National Park's tracks, then exhale as you wrap yourself in the 360-degree relaxation of one of Noosa's beauty rooms or heavenly day spas. Or book a mobile masseuse in the privacy of your holiday accommodation.
For the ultimate in relaxation, yoga in Noosa has it covered. We've got it hot and steamy, near the river, on the beach, and we have yoga that comes to you … we even have yoga on a stand-up paddle board!
Take your training to a new level with a tailored holiday fitness program from a personal trainer or at a local gym – triathletes love Noosa as a training ground and so will you.
Explore beyond the beach with Noosa Country Drive – create your own touring route and discover the beautiful nearby Noosa hinterland, its friendly villages, mountain lookouts, walking and riding trails and unique activities.
Find out where to pat an alpaca, join a cheese-making class, visit a blacksmith's sound garden, enjoy a high tea or cold brewhouse beer, browse retro relics and antiques, pick your own strawberries, go abseiling, learn how to spin your own beautiful fabric or find fresh produce at a farm gate.
If you're looking for a quiet, country getaway there's accommodation from glamping under the stars, lakefront cottages and rustic cabins to secluded B&Bs, health retreats and pub rooms.
Stop for a picnic by a tranquil lake, go bird-watching or horse riding on the Noosa Trail Network or glide through the tranquil Noosa Everglades.
See visitnoosa.com.au/country-drive and start your Noosa Country adventure!
Whether Noosa is your favourite annual holiday destination, holds happy childhood memories or you're yet to discover her enchanting ways, you'll find timeless treasures and always something fresh. Check out these new experiences next time in Noosa.
Providore on Hastings in the Netanya Noosa lobby has gourmet groceries, coffee and takeaway meals – everything for the perfect cheese platter or Noosa beach picnic.
Moto in Noosa Junction has custom bikes, surf culture, craft beers, great food and coffee from morning to late, and live beats on Sunday afternoons.
The Sofitel Noosa Pacific Resort brings French luxury to Hastings Street, rebranded from the Sheraton Noosa Resort & Spa. It's also home to Peter Kuruvita's Noosa Beach House Restaurant.
Grab Rock – literally! See amazing views from Noosa's Mt Tinbeerwah before you abseil down the rock face with half-day adventures, sunset abseils or a Rock n Surf experience.
Bordertown Barbeque and Taqueria in Gympie Tce, along the Noosa River in Noosaville has food inspired by the USA's southern states and across the border in Mexico, craft beer and …. a Bloody Mary buffet on the Acapulco Deck.
Wasabi Restaurant and Bar now has a cooking school along the Noosa River with classes and workshops covering Contemporary Japanese, Classic French, Modern South East Asian, French Patisserie, Artisan Bread Making, Preserving and Pickling, and Tea Appreciation.
Buddha on Hastings is a new restaurant and late-night lounge bar upstairs in Bay Village, with an Asian-inspired fit-out and menu by Chef Joo.
Cruise Noosa and hire a bike, scooter, four-wheel drive or classic Moke from 2Hire Moke and Scooter in Noosa Heads.
On the eastern beaches, Chalet & Co is breathing new life into a much-loved spot in Sunrise Beach with yummy breakfasts, brunch, smoothies and juices.
Experience the dramatic coastline, scenery and wildlife as you escape the bitumen and discover the sand dunes with Great Beach Drive 4WD Tours from Noosa to Rainbow Beach.
Love your craft beer? After a morning in the surf, refresh and check out Bonsai Brewery in the hinterland town of Pomona, or relive Eumundi's local beer brand which will once again be brewed at the Imperial Hotel in Eumundi from the New Year, thanks to a partnership with Lion.


text:
Q: How to create a pull to refresh tableview / scrollview in titanium? Since last 2 days i have been searching how to implement this Pull to Refresh thing like they had shown in Tweetanium.
I found some informative code snippets like
1. http://developer.appcelerator.com/blog/2010/05/how-to-create-a-tweetie-like-pull-to-refresh-table.html
But this one works only for the IOS only.
Another one is
2. https://gist.github.com/903895
This works fine with android but it has limitation that every row must be given a predefined height.
If I am getting the content to put in Row form some random JSON response then in that case I can not predefine the height of ROW in table. Thus I cannot calculate the height for the table and breaking the code.

A: Late answer, but for the next people, if you use Alloy (and you should!) http://alloylove.com/#pulltorefresh is an excellent solution.

redpajama_set_name: RedPajamaStackExchange


text:
Panel is Whoopi, Joy, Sunny, Sara, Meghan
https://www.youtube.com/watch?v=iNj1C37KcHQ
More behind the cut
Hot Topic Hot Topic #Impeachapalooza 2: The Coup d'état™
https://www.youtube.com/watch?v=eU91wESDR5w
House meets today for impeachment vote. Panel supports impeachment but unity won't occur without accountability.
MAM says blah blah. More talk about GOP wanting unity after however many just voted down certification of a free and fair election and a week after T45 incited insurrection against our own government. Clowns.
Hot Topic Pramila Jayapal
https://www.youtube.com/watch?v=kmagjtlvg2Q
https://www.youtube.com/watch?v=NHI7XZ_M3ko
Pramila Jayapal (D-WA) talks about the insurrection also being a super spreader, she has covid and started experiencing symptoms on Sunday. She's sure about when and how she got it because of her negative vs positive test timeline. Talks about penalties for Congress who refuse to wear mask. Fines are in place but doesn't go far enough. Members shouldn't be allowed on the Chamber floor or hearing rooms without mask. She explains her experience during the siege and the photo that shows her not wearing covid mask. They were told to take them off in preparation of putting on a gas mask because you can't breathe with both types of mask on. They talk about possibility of fellow Congress being co-conspirators organizing the insurrection. Bombs at RNC and DNC were planted to divert support away from the Capitol.
They move on to impeachment. Wonders about McConnell influence on Senate votes. They talk about expelling complicit Congress. 14th amendment should apply specifically to insurrectionists and those who incite violence.
Hot Topic The Joy of Reading
https://www.youtube.com/watch?v=H38f9EWZnnk
Kyle Zimmer of Disney is promoting the 30th anniversary of First Book campaign "The Magic of Storytelling" that will provide books to under-serviced children across the country. Go to www.firstbook.org for more info. So far delivered 250M books over the course of the initiative. This year, as part of the campaign, 1000 books in each panel member name will be sent to a local non profit charity of their choice.
IMPEACHMENT 2 IS COMPLETE
Democrats 222 Yes 0 No
Republicans 10 Yes 197 No 4 NV
Total 232 Yes (> needed 218)
Ontd one more week. Hugs if you're feeling overwhelmed
Source links are below each video or section
lyrics https://lyrics.az/bee-gees/allsongs.html
lyrics https://lyrics.az/future/future/mask-off.html
lyrics https://lyrics.az/hawk-nelson/diamonds/live-like-youre-loved.html
lyrics https://lyrics.az/a-boogie-wit-da-hoodie/artist/jungle.html
lyrics https://lyrics.az/kygo/-/i-see-fire-shota-edit.html


Robert Janover's wonderful and creative imagery of this beautiful Northern California region, the timely and valuable listing of the County's events, and the clean and crisp layout of each month with multiple photographs, provides an excellent representation of The County. Stunning vistas, the flowing waterscapes and towering Redwoods, the rolling vineyards, and the multitude of other outstanding places that are treats for the eyes, are all presented here to be appreciated throughout 2006! This 2006 Wall calendar was published by True Images Photography.
Select your favorite 2013 calender from our thousands of choices including our Sonoma County Calendars assortment. Our calenders include almost every type of Wall Calendar, Daily Boxed Calendar, Desk Calendar, Engaement Calendar and more. We hope you like the selection of Wall Calendars.


The rooms of this category are assigned exclusively for single and double occupancy (extra bed could not be set in the room). The total space including bathroom and small hallway is 17.5 sq.m. The classical design of the rooms is prominent due to the furnishings of beautiful natural wood with handicraft decorations of Italian master hand and makes the rooms respectable. Each room of this category has the view to Piatnitskiy side-street.
King-size bed (160 х 200 sm), two bedside drawers with individual light, in-built wardrobe with individual electronic safe inside (additional pillows and duvet), fridge (mini-bar), tea & coffee facilities, decorative mirror, armchair(s), desk with chair, satellite television and TV (21") with remote control, split air conditioner with individual remote control, luggage stand.


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Northern Ireland Press Release England Policy Wales News Position Statement UK Service Delivery Working in EM College News Joint Statement Scotland Quality Clinical Guidelines ACPs Training Coronavirus Safety Research Exams Events Safety Alerts Membership Improvement International Policy
Urgent and Emergency Care System in South West in crisis ahead of 'looming' winter
Responding to the latest Emergency Department performance figures for the South West Region, Dr James Gagg, South West Regional Chair of The Royal College of Emergency Medicine, said:
"The data for the South West is shocking. Large numbers of patients facing extremely long waiting times. The reality on the ground is awful, ambulances queuing outside packed Emergency Departments with no beds in which to move patients. Patients waiting in inappropriate places such as corridors. The situation is bleak. This is at a time of year where Health & Social Care Systems historically function better ahead of the recurring winter crises.
"Emergency Medicine staff, along with paramedics and ambulance staff, are doing all they can to ensure the urgent and emergency care system continues to function and deliver to care. But it is extremely challenging. The lack of adequate social care makes it difficult to discharge patients in a timely way. These vulnerable patients reside in hospital longer than medically necessary, unable to return to home. This causes exit block and poor flow throughout the hospital, and means we are unable to admit patients to a bed. Patients are anxious and frustrated by the long waiting times, staff are distressed at their inability to provide the quality of care they are trained to provide and face moral injury daily.
"We must get to grips with this crisis. We urge local MPs in the South West, local councils and local authorities to acknowledge this crisis and the looming winter, and act now before it is too late. We urge that social care is resourced and expanded to help with the timely discharge of patients. We ask Members of Parliament to urge the new Prime Minister, Liz Truss, and the new Secretary of State for Health and Social Care, Therese Coffey, to address the shortfall in beds and NHS staff in the South West. The scale of patient harm is distressing and completely unacceptable. As we approach winter it is critical that we mitigate this harm and keep patients safe."
The latest regional monthly performance figures published by NHS England for August 2022 for the South West show:
There were 113,686 attendances at major Emergency Departments in the South West
This accounted for 8.7% of all attendances in England
Four-hour performance at major Emergency Departments was 54.8%
This means that 51,836 patients spent a minimum of four hours in a major Emergency Department, equal to just over one in two attendances
3,721 patients were delayed for 12 hours or more from decision to admit to admission
This figure was 648 in August 2021, and was just 22 in August 2019
There were 31,836 emergency admissions to hospital to major (Type 1) Emergency Departments
This means that more than one in nine patients admitted to a major Emergency Department were waiting for 12-hours or more