text:
\section{Introduction}\label{intro}
The earliest stages of low-mass star formation are now reasonably well understood. Stars are known to form within molecular clouds, or more precisely, within prestellar cores \citep{1994MNRAS.268..276W,1996A&A...314..625A,1999MNRAS.305..143W}, which are the density peaks of the molecular cloud that have become gravitationally bound. The youngest stars that have been observed are the Class 0 protostars \citep{1993ApJ...406..122A,2001A&A...369..155C}, which are still accreting material from their surrounding envelope. This envelope is the remnant of the prestellar core within which the protostar was born. For a detailed review of this process, see \citet{2000prpl.conf...59A,dwt_ppv}.

However, the formation mechanism for the lowest mass stars and brown dwarfs is less well understood, partially due to the observational difficulties in imaging these low-mass objects. Given the assumption that the minimum mass of a star that forms by the gravitational fragmentation of a molecular cloud is the Jeans mass \citep{1992MNRAS.256..641L}, it has been suggested that these very low-mass objects form by a different mechanism to solar-mass stars. There have been a number of mechanisms suggested, including star formation in low-mass cores that are created in shock compressed layers \citep[e.g.][]{2005A&A...430.1059B}, or ejection from a more massive core before it has time to accrete very much mass \citep{2001AJ....122..432R,2002MNRAS.332L..65B,2002MNRAS.336..705B,2004A&A...414..633G,2004A&A...419..543G,2004A&A...423..169G}. These mechanisms and others are reviewed in \citet{ant_ppv}.

A recent important observational result in the study of star formation is the discovery that the mass spectrum of prestellar cores mimics the Salpeter-like power-law slope of the stellar initial mass function at high masses \citep{1998A&A...336..150M}.
However, due to completeness limits, neither this nor more recent studies have probed the relation between the core mass function (CMF) and the stellar IMF at low masses. Knowledge of the relation between the CMF and the IMF in this mass regime is required to understand the formation mechanism of very low-mass stars and brown dwarfs.

The Orion molecular cloud is the closest high mass star-forming region \citep[][and references therein]{1989ARA&A..27...41G}. The distances to the front and rear edges of the Orion molecular cloud were determined by \citet{1994A&A...289..101B} to be $\sim 320$ pc and $\sim 500$ pc respectively. We therefore assume a canonical distance to the Orion star-forming regions of 400 pc.
The molecular cloud is composed of two parts. The Orion A cloud (L1640/1641) is located in the southern half of the Orion constellation. It contains OMC1, which is the most active site of current star formation in the region, and houses the Trapezium cluster of O and B stars. The Orion B cloud (L1630) lies approximately 5 degrees (35 pc) north of Orion A and is made up of two sub-clouds. The Orion B South cloud contains the star-forming region NGC 2023/2024, and is the formation site of the only O stars in Orion B. This part of the cloud is the location of B33, the famous Horsehead nebula \citep[see][and references therein]{2006MNRAS.369.1201W}. Orion B North is located 2.5 degrees (17 pc) north of NGC 2024, and contains the NGC 2068/2071 and HH24-26 star-forming regions. The Orion molecular cloud is illustrated in Figure~\ref{orion_overview} which shows the IRAS 100~$\mu$m data \citep{IRAS} produced using the {\em skyview} interface \citep{1994ASPC...61...34M}, along with the regions that have been mapped in the submillimetre.

In this study, we have combined all of the SCUBA wide-field scan-map data taken to date of the Orion molecular cloud, to produce the deepest and widest-area submillimetre maps of this cloud. With these data, we investigate the low-mass end of the CMF, and also compare the mass spectra for the different regions of the molecular cloud in a self consistent way. We further provide a catalogue of the size and mass of each of the detected cores within the Orion molecular cloud.

\begin{figure}
\includegraphics[angle=0,width=83mm]{./fig1.eps}
\caption{IRAS 100~$\mu$m map of the Orion molecular cloud \citep{IRAS}, as well as the familiar stars of the constellation. The north-south extent of the image is 20 deg, which at an assumed distance of 400 pc, corresponds to 140 pc. The extents of the four regions that have been mapped in the submillimetre are outlined in black. Our names for these regions are labelled.}
\label{orion_overview}
\end{figure}

\section{Observations}\label{observations}
The submillimetre data presented in this study were obtained using the Submillimetre Common User Bolometer Array (SCUBA) on the James Clerk Maxwell Telescope (JCMT). This instrument takes observations at 450 and 850~$\mu$m simultaneously through the use of a dichroic beam-splitter. The telescope has a resolution of 8 arcsec at 450$~\mu$m and 14 arcsec at 850~$\mu$m. The data presented here were acquired from the JCMT data archive, operated by the Canadian Astronomy Data Centre. Sub-sets of these data have been published previously \citep{1999ApJ...510L..49J,JohnstoneOriAS,2001ApJ...556..215M,2001A&A...372L..41M,2001ApJ...559..307J,2006ApJ...639..259J,2006MNRAS.369.1201W}, though all the data have been re-reduced using a consistent method for this study.

The observations were carried out over 30 separate nights between February 1998 and March 2002 using the scan-map observing mode. A scan-map is made by scanning the array across the sky. The scan direction is 15.5$^\circ$ from the axis of the array in order to achieve Nyquist sampling. The array is rastered across the sky to build up a map several arcminutes in extent.

Time-dependent variations in the sky emission were removed by chopping the secondary mirror at 7.8 Hz. Due to a scan-map being larger in size than the chop throw, each source in the map appears as a positive and a negative feature. In order to remove this dual-beam function, each region is mapped six times, using chop throws of 30, 44 and 68 arcsec in both RA and Dec \citep{1995mfsr.conf..309E}. The dual-beam function is removed from each map in Fourier space by dividing each map by the Fourier transform of the dual-beam function, which is a sinusoid. The multiple chop-throws allow for cleaner removal of the dual beam function in Fourier space. The maps are then combined, weighting each map to minimise the noise introduced at the spatial frequencies that correspond to zeroes in the sinusoids. Finally the map is inverse Fourier transformed, at which point it no longer contains the negative sources \citep{SURF}.

\begin{figure*}
\begin{minipage}[t]{80mm}
\includegraphics[angle=0,width=80mm]{./fig2a.eps}
\end{minipage}
\begin{minipage}[t]{80mm}
\includegraphics[angle=0,width=80mm]{./fig2b.eps}
\end{minipage}
\begin{minipage}[t]{80mm}
\vspace{0pt}
\includegraphics[angle=0,width=80mm]{./fig2c.eps}
\end{minipage}
\begin{minipage}[t]{80mm}
\vspace{0pt}
\includegraphics[angle=0,width=80mm]{./fig2d.eps}
\end{minipage}
\caption{The four maps of the Orion molecular cloud at 850~$\mu$m.
a) Orion AN, with contour levels at 5, 10, 20, 40, 80 and 160$\sigma$, where $\sigma$ is the mean noise level over the whole of the map, equal to 19 mJy/beam.
b) Orion AS, with contours at 5, 10, 15, 20 and 40$\sigma$, where $\sigma$ is equal to 18 mJy/beam.
c) Orion BN, with contours at 5, 10, 15, 20 and 40$\sigma$, where $\sigma$ is equal to 16 mJy/beam.
d) Orion BS, with contours at 5, 10, 15, 20 and 40$\sigma$, where $\sigma$ is equal to 23 mJy/beam.}
\label{Orion_maps}
\end{figure*}

The submillimetre zenith opacity at 450 and 850$~\mu$m was determined using the `skydip' method and by comparison with polynomial fits to the 1.3~mm sky opacity data, measured at the Caltech Submillimeter Observatory \citep{2002MNRAS.336....1A}. The sky opacity at 850$~\mu$m varied from 0.12 to 0.51, with a median value of 0.26. These correspond to a 450$~\mu$m opacity range of 0.5 to 3.1, and a median value of 1.4.

The data were reduced in the normal way using the SCUBA User Reduction Facility \citep{SURF}. Noisy bolometers were removed by eye, and the baselines, caused by chopping onto sky with a different level of emission, were removed using the {\em \small MEDIAN} filter. Calibration was performed using observations of the planets Uranus and Mars, and the secondary calibrators HLTau and CRL618 \citep{1994MNRAS.271...75S} taken during each shift. We estimate that the absolute calibration uncertainty is $\pm7\%$ at 850$~\mu$m and $\pm15\%$ at 450$\mu$m, based on the consistency and reproducibility of the calibration from map to map.

The submillimetre data make up 4 separate maps. The relative positions of these maps are illustrated in Figure \ref{orion_overview}. The most northerly map of the four is centred on the northern star-forming complex in Orion B, including NGC 2071, NGC 2068 and HH24/25/26. Hereafter, we refer to this map as Orion BN. The Orion B South map (hereafter Orion BS) encompasses the southern star-forming component of Orion B, and includes NGC 2023, NGC 2024 and the Horsehead nebula (B33). The Orion A cloud is also made up of two maps, the northernmost of which (Orion A North -- hereafter Orion AN) includes OMC 1, 2 and 3. Directly to the south of Orion AN is Orion A South (hereafter Orion AS), which follows the Orion A filament to the south-east. The area covered by each of the maps is given in Table~\ref{noise_levels}.

The 850~$\mu$m data for the four regions are shown in Figures \ref{Orion_maps}(a-d). These figures show that the data contain a large number of dense cores, which are usually associated with larger scale filamentary structure. The main difference in the general morphology of the different regions is that they vary in richness, for example the cores in the Orion AN map are more numerous and more closely packed than in the other three regions.

\section{Results}\label{results}
\subsection{Submillimetre continuum data}
In order to produce the deepest maps possible, the data are made up from a number of different observing programs, therefore the map coverage is not uniform for each region. In addition, the weather conditions varied when the data were taken. As a result, the noise levels vary across each map. In order to quantify the variation of the noise level across the map, a noise-map was generated using the following technique.

The bright sources in the map were masked in order to prevent the rapid change in flux density at the positions of these sources from contaminating the noise estimate. For the same reason, the large scale structure of the map was removed by smoothing the map and subtracting this from the data. The noise-map was then built up by measuring the standard deviation of the resulting data at each point in an aperture of radius 50 arcsec. The gaps in the noise-map caused by the masking of the bright sources were filled in by interpolation from the surrounding regions.

To illustrate this, the noise-map for the Orion BN is shown in Figure \ref{Orion BN_noisemap}, where the grey scale indicates the noise level in the map. As can clearly be seen, the noise level is lower towards the centre of the map due to increased coverage by the different observing programs. This effect is seen in all of the different regions. Table~\ref{noise_levels} gives the average noise levels, measured using the noise-maps. The quoted value corresponds to the average noise level measured over all parts of the map which contain detected sources. For comparison, previous authors using different subsets of the SCUBA data of Orion have found values for the 1$\sigma$ 850~$\mu$m noise level in the range $22-40$ mJy/beam \citep{1999ApJ...510L..49J,JohnstoneOriAS,2001A&A...372L..41M,2001ApJ...559..307J,2006ApJ...639..259J}.

\begin{figure}
\includegraphics[angle=0,width=83mm]{./fig3.ps}
\caption{The 850~$\mu$m noise-map for the Orion BN region. Contours are 10, 15, 20, 30, 40, 50, 60 \& 70 mJy/beam. See text for details.}
\label{Orion BN_noisemap}
\end{figure}

\begin{table}
\begin{center}
\caption{The statistics for each of the four mapped regions. The number of cores detected in each region is given in column 2. The average 1$\sigma$ noise levels for the 850~$\mu$m and 450~$\mu$m data are given in columns 3 and 4 respectively. The 450~$\mu$m noise level is based on the data after smoothing to the 850 $\mu$m resolution.}
\label{noise_levels}
\vspace{0.5cm}
\begin{tabular}{ccccc} \hline
Cloud 		& Map		& No. of	& \multicolumn{2}{c|}{1$\sigma$ noise level} 	\\
Name 		& Area		& cores		& 850~$\mu$m	& 450~$\mu$m		\\
		& (sqdeg)	&		& (mJy/beam)	& (mJy/beam)		\\ \hline
Orion AN	& 0.23		& 172		& 19		& 67			\\
Orion AS	& 0.41		& 62		& 18		& 60			\\
Orion BN	& 0.32		& 100		& 16		& 39			\\
Orion BS	& 0.45		& 59		& 23		& 68			\\ \hline
\end{tabular}
\end{center}
\end{table}

In order to extract the properties of each core in a consistent manner across all of the maps, each map was divided by the noise-map described above, to produce a signal to noise (S/N) map. The significance and dimensions of sources were determined using this S/N map using the following criteria.

A source was deemed real if it had a peak flux density $> 5\sigma$ relative to the local background. Close peaks were separated into two sources if the difference between the peak of the weaker source and the minimum between the sources was $> 3\sigma$. Elliptical apertures were placed on each source and approximately matched to the position of the $3\sigma$ contour. The flux density for each source was then determined by placing the aperture, defined using the S/N map, on the original data. In each case the flux density was measured relative to the local background level by placing a `sky' aperture on a nearby blank area of the map. The number of cores detected in each region is given in Table~\ref{noise_levels}, and the properties of each core are listed in Table~\ref{cores_table} in Appendix~A.

\begin{figure*}
\begin{minipage}[t]{80mm}
\includegraphics[angle=270,width=80mm]{./fig4a.ps}
\end{minipage}
\begin{minipage}[t]{80mm}
\includegraphics[angle=270,width=80mm]{./fig4b.ps}
\end{minipage}
\begin{minipage}[t]{80mm}
\vspace{0pt}
\includegraphics[angle=270,width=80mm]{./fig4c.ps}
\end{minipage}
\begin{minipage}[t]{80mm}
\vspace{0pt}
\includegraphics[angle=270,width=80mm]{./fig4d.ps}
\end{minipage}
\caption{The core mass functions for the four mapped regions. The solid histogram includes all cores that were detected at 850 $\mu$m. The dotted histogram shows only those cores which do not contain a Class I protostar, as determined using mid-IR Spitzer data. The error bars are the statistical error due to the number of cores in each bin. The dotted and dashed vertical lines show the 5$\sigma$ sensitivity and completeness limit respectively for each region. All detected submillimetre sources are included in these mass functions.}
\label{Orion_CMFs}
\end{figure*}

This strategy for characterising individual cores was applied to each source in the data with the exception of those sources that are embedded in a large amount of extended emission and are very close to neighbouring sources. In the case of these sources, their proximity to their neighbours means that the aperture size is necessarily reduced relative to the $3\sigma$ defined aperture discussed above. In order to compensate for this effect, the surrounding extended emission above the $3\sigma$ contour was partitioned between the cores relative to their peak flux density.

Due to the poorer atmospheric opacity at 450~$\mu$m, the sources in the 450~$\mu$m data have significantly lower signal to noise ratios compared to the 850~$\mu$m data. The 450~$\mu$m data were therefore smoothed such that the FWHM resolution matched that of the 850~$\mu$m data. The sources were then extracted from the 450~$\mu$m data in a similar manner to that described above, with a signal to noise map being generated for each region, and a detection criterion of 5$\sigma$ applied. Each source that was detected at 450~$\mu$m has a corresponding detection at 850~$\mu$m, though not all sources that were detected at 850~$\mu$m were detected at 450~$\mu$m. The integrated flux was measured for the sources that were detected at 450~$\mu$m using apertures with the same position and dimensions as those used for the 850~$\mu$m sources. This is to allow a direct comparison of the data at the different wavelengths. The 450~$\mu$m properties for each core are given in Table~\ref{cores_table} in Appendix~A.

\subsection{Spitzer IRAC results}
Mid-IR data for the four regions taken using the IRAC camera \citep{2004ApJS..154...10F} on board the Spitzer space telescope were retrieved from the Spitzer data archive. These data have wavelengths of 3.6, 4.5, 5.8 and 8.0~$\mu$m. The data were calibrated using the IRAC science BCD pipeline prior to retrieval from the archive \citep{IracHandbook}.

Each waveband of the IRAC data was independently searched for point sources that lie within the 3$\sigma$ contour of the submillimetre detected cores. The flux density of each source was measured in a circular aperture, the position and size of which was fixed for all wavelengths. Extended emission from the surrounding cloud was removed using an off-source `sky' aperture. The magnitudes of the sources were calculated using the zero magnitude flux densities given in the Spitzer Observer's Manual \citep{SpitzerUserGuide}.

Sources that were detected in all 4 IRAC bands were classified as Class I or Class II YSOs or as stars according to their [5.8] - [8.0] and [3.6] - [4.5] colours, as described in \citet{2004ApJS..154..363A}. Sources that were detected in either 2 or 3 IRAC bands, were classified according to their spectral index \citep{1987IAUS..115....1L}. Submillimetre sources that contain a Class I YSO were removed from our sample to remove protostellar contamination of the pre-stellar core statistics.

\section{Core Mass Functions}

The masses of the cores are calculated from their 850~$\mu$m integrated flux density, which is assumed to be optically thin. The core mass is calculated using the following:
\begin{equation}
M=\frac{S_{850}D^2}{\kappa_{850}B_{850,T}},
\end{equation}
\noindent
where $S_{850}$ is the 850~$\mu$m flux density, $D$ is the distance to the source, $\kappa_{850}$ is the mass opacity of the gas and dust, and $B_{850,T}$ is the Planck function at temperature $T$. We assume a distance to the region of 400 pc \citep{1994A&A...289..101B}, a temperature of 20~K for the Orion cores \citep{1996A&A...312..569L,2001ApJ...556..215M,2006ApJ...639..259J}, and a mass opacity of ${\rm 0.01~cm^2g^{-1}}$ \citep[see][for a detailed discussion of both this value of $\kappa_{850}$ in particular and of this method of obtaining masses in general]{1993ApJ...406..122A,1996A&A...314..625A,1999MNRAS.305..143W}. We note that the assumption of a single temperature for all of the cores could potentially introduce a systematic bias in the calculated mass if there is a correlation between the temperature and mass of the cores.

The core mass functions for the four regions are shown in Figures \ref{Orion_CMFs}(a-d). The error bars shown are the $\sqrt{N}$ counting uncertainty due to the number of cores in each mass bin. The dotted vertical lines show the $5\sigma$ sensitivity of the map. This is based on the average noise level as shown in Table~\ref{noise_levels}, and converted to a mass using the assumptions of distance, temperature and dust opacity given above. This signifies the minimum detectable point source in the map. The dashed lines show the $5\sigma$ completeness limit of the maps. The completeness limit is higher than the sensitivity because an extended source with a $5\sigma$ peak flux density is more massive than a point source with the same peak flux density. These figures show that our data are consistent with previous studies.

Given the selection criteria discussed in the previous section, the completeness limit for a given noise level ($\sigma$) and source size ($r_{eff}$) can be estimated by measuring the fraction of the total flux density that is contained within an aperture set at 3/5 of the peak flux density, for a number of sources in the data. This fraction can then be applied to a source at the limit of the detection (i.e. a peak flux density equal to $5\sigma$), and gives the flux density that is contained within the $3\sigma$ contour. The source size ($r_{eff}$) is defined to be the radius that defines a circle with the same area as the elliptical aperture placed on the source. $\overline{r}_{eff}$ is calculated independently for each region and is taken to be the average size of the detected low-mass sources (based on the lowest mass one third of the sources). The low-mass sources are selected as being more representative of the average source size at the limit of detection.

\begin{figure*}
\begin{minipage}[t]{80mm}
\includegraphics[angle=270,width=80mm]{./fig5a.ps}
\end{minipage}
\begin{minipage}[t]{80mm}
\includegraphics[angle=270,width=80mm]{./fig5b.ps}
\end{minipage}
\caption{a) The core mass function for the Orion BN region, plotted as a cumulative mass function to allow comparison with fig.~3 of \citet{2001A&A...372L..41M}. The Class I YSOs identified through the IRAC data have been removed from the data. The fits from \citeauthor{2001A&A...372L..41M} of $N(>m) \propto m^{-0.6}$ and $N(>m) \propto m^{-1.35}$ are shown as dotted and dot-dashed lines respectively. b) The same data, plotted as an unbinned cumulative mass function for comparison with fig.~8 of \citet{2001ApJ...559..307J}. All submillimetre detected sources are plotted. The fits from \citeauthor{2001ApJ...559..307J} of $N(>m) \propto m^{-0.5}$ and $N(>m) \propto m^{-1.5}$ are shown as dotted and dot-dashed lines respectively. The dotted line shows the position of the completeness limit.}
\label{OriBN_comparisons}
\end{figure*}

\begin{table}
\begin{center}
\caption{The point source sensitivity, completeness limit and average effective radius ($\overline{r}_{eff}$) for each of the four regions. $r_{eff}$ is based on the lowest mass 1/3 of the sources in that region.}
\label{table_stats}
\vspace{0.5cm}
\begin{tabular}{cccc} \hline
Cloud 		& $5\sigma$	& $\overline{r}_{eff}$	& Completeness 	\\
Name 		& sensitivity	& (arcsec)		& limit		\\
		& ($M_{\odot}$)	& 			&($M_{\odot}$)	\\ \hline
Orion AN	& 0.15		& 14			& 0.29		\\
Orion AS	& 0.13		& 16			& 0.37		\\
Orion BN	& 0.12		& 16			& 0.31		\\
Orion BS	& 0.17		& 17			& 0.45		\\ \hline
\end{tabular}
\end{center}
\end{table}

The relation between the completeness limit and the core mass function is insensitive to the assumptions of distance, temperature and dust opacity, discussed in the previous section, because both the core masses and the completeness limit scale in the same way if these assumptions are adjusted. The point source sensitivity, completeness limit and effective radius for each of the four regions are given in Table~\ref{table_stats}.

Looking at the Figures \ref{Orion_CMFs}(a-d), a number of features are apparent. The high mass side of the mass function declines as a power-law to higher masses, in agreement with previous studies of both Orion and other star-forming regions \citep{1998ApJ...508L..91T,1998A&A...336..150M,2001A&A...372L..41M,2001ApJ...559..307J,2002ApJ...575..950O,2006ApJ...639..259J}. The low-mass side of the mass function also declines to lower masses, and for two of the four regions mapped (Orion AN and Orion BN), this decline begins at significantly higher mass than the completeness limit. The peak of the core mass functions for these two regions show a peak in the mass bin that is centred on 1.3~$M_{\odot}$. This is a factor of 4 larger than the average 5$\sigma$ completeness limit of the two regions.

We therefore believe that this is a real effect, and signifies the discovery of the turn-over in the core mass function. The physical significance of this is discussed in the following section. A third region (Orion AS) is also consistent with this picture, with the mass function appearing to turn over before the completeness limit is reached. However, there are a smaller number of sources detected in this region, and so there is more scatter in the different bins of the mass function. This causes the position of the peak of the mass function, and hence the significance of the turn-over, to be less certain. In the fourth region (Orion BS), there are a similarly small number of sources as in Orion AS. Also, the completeness limit is a factor of 1.5 times higher than in Orion AN and Orion BN. In this region there appears to be no significant decline in the number of cores until the completeness limit is reached.

As one would expect, there are no sources with a lower mass than the sensitivity limit, and in the mass functions for the Orion AN and Orion BN regions, there is a sharp decline in source numbers at the level of the completeness limit, lending support to our estimate of the completeness.

Subsets of these data for the Orion BN region have been published previously \citep{2001ApJ...559..307J,2001A&A...372L..41M}. In order to allow easy comparison with these earlier works, mass functions for the Orion BN data are plotted in Figures~\ref{OriBN_comparisons}a \& b in the same cumulative form as that used in the earlier papers. The plotted fits to the data have the same slopes as are shown by \citeauthor{2001ApJ...559..307J} and \citeauthor{2001A&A...372L..41M} respectively. Though our data are complete to lower masses, Figures~\ref{OriBN_comparisons}a \& b show that the data presented here are consistent with the earlier work.

\begin{figure}
\includegraphics[angle=270,width=83mm]{./fig6.ps}
\caption{The core mass function for the Orion AN and Orion BN regions. The average completeness limit for the two regions is shown as a dashed line. A three-part stellar IMF, normalised to the peak in N of the CMF, is overlaid as a thin solid line. The dotted line shows a three-part mass function with the same slopes as the IMF (see text for details).}
\label{comparison_imf}
\end{figure}

\section{Discussion}
In the previous section we demonstrated that the core mass functions for the two regions Orion AN and Orion BN turn over at a significantly higher mass than the completeness limit of the data. In Figure~\ref{comparison_imf}, we combine the data for these two regions and plot the resulting CMF on a log-log plot.

The low-mass side of the CMF is best fitted by a power-law of following the form:
\begin{equation}
M\frac{dN}{dM} \propto M^{-x}
\label{imf1}
\end{equation}

where $x$ is equal to $-0.35 \pm 0.2$ between the completeness limit at ${\rm \sim 0.3 M_\odot}$ and the peak at ${\rm \sim 1.3~M_\odot}$. At higher masses than the peak, we find that the CMF is best fitted by a power-law with $x$ equal to $1.2 \pm 0.2$.

We compare this CMF with the stellar IMF, for which we assume a three-part power-law form with the following exponents:
\begin{equation}
\begin{array}{lcrrll}
x & = & 1.35,  & 0.5~M_{\odot}  &<~M,~& \\
x & = & 0.3,   & 0.08~M_{\odot} &<~M~<& 0.5~M_{\odot}, \\
x & = & -0.3,  & ~~~~~~0.01~M_{\odot} &<~M~<& 0.08~M_{\odot}.
\end{array}
\label{imf2}
\end{equation}
Above the peak of the IMF at $0.08~M_\odot$, the power-law slopes of the IMF are those observed for field stars, taken from \citet{2002Sci...295...82K}. Below $0.08~M_\odot$, the IMF is based on fits to the stellar populations of young clusters \citep{2003PASP..115..763C}. These clusters are observed to have power-law slopes varying between 0.2 and 0.4, therefore an average value of $0.3 \pm 0.1$ is used here. This IMF is plotted on Figure~\ref{comparison_imf} as a thin solid line.

The Orion CMF plotted in Figure~\ref{comparison_imf} is consistent with a mass function with the same slopes as the three-part power-law IMF given in Equations \ref{imf1} and \ref{imf2}, between the following masses.
\begin{equation}
\begin{array}{lcrrll}
x & = & 1.35,  & 2.4~M_{\odot}  &<~M,~& \\
x & = & 0.3,   & 1.3~M_{\odot} &<~M~<& 2.4~M_{\odot}, \\
x & = & -0.3,  & ~~~~~~0.4~M_{\odot} &<~M~<& 1.3~M_{\odot}.
\end{array}
\label{imf3}
\end{equation}
This three-part power-law is plotted as a dotted line on Figure~\ref{comparison_imf}.

There are a number of similarities and differences between the CMF and the IMF shown in Figure~\ref{comparison_imf}. Both mass functions are well fit by negative power-law slopes at large masses, and decline to lower masses below a peak value. The most obvious difference between the two mass functions is that the turn-over of the CMF occurs at a much higher mass (${\rm \sim 1.3~M_\odot}$) than that of the IMF (${\rm \sim 0.08~M_\odot}$).

If we were to assume a simple 1:1 mapping of the CMF to the IMF, whereby each core forms a single star, then these data show that the star formation efficiency (SFE) is only $\sim 6\%$ within the gravitationally bound core. The measured SFEs for star-forming regions are typically much larger, at $\sim 30\%$ \citep[][and references therein]{2003ARA&A..41...57L}. This discrepancy could be explained by the formation of multiple stars within each core.

The best fit power-law to the low-mass slope of the IMF has an exponent of $0.35 \pm 0.2$. This is consistent with the low-mass slope of the stellar IMF for young clusters which is observed to lie between 0.2 and 0.4 \citep{2003PASP..115..763C}. We compare the CMF to the IMFs of these systems because being so young, any causal relation is more likely to be apparent. The slope of the low-mass side of the CMF is based on only three data-points, and must therefore be considered a tentative result. However, if it is borne out to be correct by future observations, then it shows that the CMF continues to mimic the stellar IMF down to very low masses. We also note that a study of the nearer, lower-mass cloud $\rho$-Ophiuchi does not show a turn-over in the core mass function, down to their completeness limit of $\sim 0.1~M_\odot$ \citep{1998A&A...336..150M}. It is therefore possible that the position of the turn-over in the CMF varies as a function of environment.

\section{Conclusions}
We have combined all of the wide-field SCUBA data of the Orion molecular cloud from the JCMT archive, in order to create the deepest and most extensive maps of this region to date. We have extracted the cores from these data, and generated core mass functions for each region. We have estimated the completeness limit of each map, based on the sensitivity limits of the data and the average size of the low-mass cores. We find that for two of the regions, Orion A North and Orion B North, the CMF turns over at a significantly higher mass than the completeness limit. This marks the discovery of the turn-over of the CMF. We compare the CMF to a canonical stellar IMF, and find that the turn-over in the CMF occurs an a much higher mass than in the IMF. We find that the CMF is best fit by power-laws with exponents of 0.35 between 0.3 and 1.3 M$_\odot$, and -1.2 above 2.4 M$_\odot$. The CMF is consistent with the power-law slopes of the stellar IMF down to the completeness limit of the data.

\section*{Acknowledgements}
This research is based on observations obtained with the James Clerk Maxwell Telescope, which is operated by the Joint Astronomy Centre in Hilo, Hawaii on behalf of the parent organizations PPARC in the United Kingdom, the National Research Council of Canada and The Netherlands Organization for Scientific Research. The data were obtained using the Canadian Astronomy Data Centre, which is operated by the Herzberg Institute of Astrophysics, National Research Council of Canada. The observations were taken under the programs M98AC19, M98BC14, M98BH01, M98BN06, M98BU55, M99BC27, M99BC30, M00BC10, M00BC15, M01AC10 and M02AC32. The authors would like to thank the staff of the JCMT for assistance with the observations. This work is also based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. DN acknowledges PPARC for PDRA support. This work was carried out while DWT was on sabbatical at the Observatoire de Bordeaux and at CEA Saclay, and he would like to thank both institutions for the hospitality accorded to him.


Veii is the second instalment, after Caere, of the University of Texas Press' new series "Cities of the Etruscans." The book under review was edited by Jacopo Tabolli, who has excavated at the site of Veii for some time now. Chapters were authored by many prominent figures in both the study of the city itself and Etruscology more generally. The papers are divided into four distinct parts which focus on different aspects of Veii.
Part I looks at the archaeology of the city. Valeria Acconcia opens with a study of the Piazza d'Armi plateau which is south of the main plateau of the city. This includes a history of excavations on the site and discussion of what this history of examination can tell us about settlement in this part of Veii. This began in the ninth century BC and continued through to the early fifth century. She outlines a four-phase history of occupation. Amongst the discoveries noted are the hut burial, so-called oikos (temple), and the monumental cistern. Importantly, Acconcia notes that the fortifications once dated to the sixth century BC are actually medieval, of the ninth to eleventh century AD.Show A full discussion of this major reconsideration can be found in G. Bartoloni and L. Pulcinelli, "Veio. Le mura di Piazza d'Armi," in P. Fontaine and S. Helas (eds.), Fortificazione arcaiche del Latium vetus e dell'Etruria meridionale (2016).
The second chapter discusses the surveys that have been conducted in Veii and its hinterland. Roberta Cascino takes us through Ward-Perkins' work from the 1950s to more recent work of this type. The importance of these projects is shown by how they have illuminated our understanding of the city's settlement history.
Stefano Campana closes out Part I with an overview of an ongoing project to examine the Veii plateau via magnetic survey. This is still a work-in-progress, but this chapter shows its promise. We mostly hear about the results as they pertain to the city's road system, which originated in the Iron Age, i.e. early in the settlement's history. It consisted of two major arterial roads and numerous collector roads which connected the various residential and public areas within the city to the major thoroughfares. Magnetic survey has also supported the results of earlier field walking surveys, which helps instill confidence in broader arguments made using them as evidence.
Part II of the book is dedicated to the history of Veii. It includes thirteen chapters which consist of narrative discussions, such as Folco Biagi's paper on Veii from the Final Bronze Age to the Early Iron Age, and topical discussions, such as Francesca Boitani's "Veii and the Greeks." The chapters in this section provide a thorough overview of the development of the city, its territory, and its relations with its neighbors and those further afield.
We begin with the earliest visitation and habitation of the plateau which made up the later city. Humans have been active in the area since the paleolithic, but only inhabited it permanently from the Early Iron Age. This is not necessarily abnormal for the sites which would become the great city-states of the region.
One of the most interesting discussions in this part of the book, at least to me, is that of Veii's territory and borders. Jacopo Tabolli's chapter, in particular, provides a very enlightening overview of the city's relations and ties to those closest to it, namely the peoples of the Ager Faliscus and Ager Capenas. He convincingly describes the Tiber basin as a cultural melting pot, in which elements of all the regional cultures can be found mixed together in different ways at the various settlements.
Part III is made up of eight chapters that look in-detail at the material culture of Veii. While this is, in general, the same type of evidence as discussed in the earlier chapters, the authors here examine specific categories on their own terms, rather than through a historical lens. Topics include pottery styles, metalwork, wall painting, sculpture, and architectural decoration. We are presented with an image of a Veii whose tastes changed rather dramatically from the Early Iron Age to the later years of its existence. This section has shown also that it was a city of production and craft, style and innovation.
Part IV is brief, consisting mostly of Christopher Smith's historical discussion of Camillus and Rome's conquest of Veii. Jacopo Tabolli and Orlando Cerasuolo's conclusion is located in this section, as well, and is followed by a helpful chronological outline of the city's history (p. 229-233). Interestingly, and conveniently, this includes the dates of archaeological projects carried out in and around Veii, ending with an entry for 2016 CE: "The Museum of the Ager Veientanus in Formello is reopened to the public with a new collection" (p. 233).
Altogether, this book presents a view of Veii that few readers of English will be used to, or even perhaps expect. The great city typically plays the role of antagonist in studies of early Rome and the details of its own life are elided. Even in surveys on Etruscan archaeology and history, it typically takes a "backseat" compared to the coastal centers such as Caere or Tarquinia. Those interested have had for some time Robert Leighton's monograph on the latter, and since 2016 the volume Caere in the same series as the subject of this review.Show R. Leighton, Tarquinia: An Etruscan City (2004).
It is impossible to discuss all the insights gained, and wonderful things explored, in this book. I wish to simply highlight a few.
Luca Pulcinelli's chapter on "The Defensive System" is very timely and thorough. The study of fortifications in Central Italy has been growing for some time, with a major volume reevaluating the chronology of some of these notable amongst the rest.Show P. Fontaine and S. Helas (eds.), Fortificazione arcaiche del Latium vetus e dell'Etruria meridionale (2016). Pulcinelli shows that he is up-to-date on this research and with this chapter has made it accessible to those who are less capable in the European languages. He rightly points to the strength of the fortifications at Veii, especially from the sixth century onward, which were all but impervious to the siege engines of the time (ladders and rams) (p. 151).
We are also enlightened about an aspect of Veii's artistic legacy which is often overshadowed by its neighbors (especially Tarquinia), and that is wall paintings. Francesca Boitani supplies us with a delightful, if short, chapter on the topic, supplemented by a number of full-color plates. She highlights one of the most interesting and charming painted tombs from Etruria, "The Tomb of the Roaring Lions." Painted in the early seventh century BC, its style is endearing and, though influenced by the Late Geometric from the Aegean, is rather unique.
Barbara Belelli Marchesini's contribution is also an interesting standout for its topic, "Kilns and Evidence of Ceramic Production." While classical archaeology has had a perennial obsession with pottery, the manufacture thereof has not always been appreciated. She covers all of the evidence for this kind of activity throughout the city, shedding light on one of the most important day-to-day activities of any ancient settlement. The discussion of the so-called Lady of the Furnaces, a single female inhumation burial in one of the earliest industrial areas (later covered by a defensive agger at the end of the ninth century BC), is refreshing, and reminds us of how little we know about specific cultural practices in the Early Iron Age. Why was this woman buried here, on the main urban plateau?
Amongst a volume of chapters that primarily deal with archaeology, Christopher Smith's paper is an interesting and enlightening discussion of the history – or myth – surrounding Rome's conquest of Veii and its territory. He focuses on the story of Marcus Furius Camillus, who is said to have led the Roman forces at the end of a fabled ten-year siege of their Etruscan neighbour. Of course, the duration of this is mythological and was created to make the first major act of aggression by Rome equivalent in scope to the Trojan War. Nevertheless, the figure of Camillus is fraught with difficulties in terms of historical interpretation. Did he actually exist? If so, is the history of his life that we possess accurate at all?
Smith addresses critical responses to the first of these questions, showing both their strengths and their weaknesses. He takes a judicious stance, in some ways conceding that we cannot side entirely with the sceptical answers, but also that the story of Camillus as we have it is at best a mythologized version of actual historical events. The conclusion that "in the end, however, we do not need to decide whether Camillus was a real person or a historicized myth in order to be able to say something about the history of Veii in the early fourth century BCE" is erudite and presents a way forward not afforded by hyper-critical approaches (p. 223).
In general, my impression of this volume is that it is an important addition to the corpus of Etruscan studies. Not only does it bring considerable research to English readers that would otherwise be unavailable, but its chapters include insightful new thoughts on their relative topics by the stellar cast of authors. It is a testament to the success of the new series from the University of Texas Press, spearheaded by the series editors Nancy Thomson de Grummond and Lisa C. Pieraccini.
Audiences of students, scholars, and general readers will find much of value in this book, and anyone with a serious interest in Etruria or early Rome should seek it out. I look forward to the future volumes and to the renewed passion for Etruscology that I hope they will instil in Anglophone students.


This Act gives States the responsibility to dispose of low-level radioactive waste generated within their borders and allows them to form compacts to locate facilities to serve a group of States. The Act provides that the facilities will be regulated by the NRC or by States that have entered into Agreements with the NRC under section 274 of the Atomic Energy Act. The Act also requires the NRC to establish standards for determining when radionuclides are present in waste streams in sufficiently low concentrations or quantities as to be "below regulatory concern."


These Swarovski glass beads are delightful and fun to wear. The perfect black and white accompaniment for any black or white outfit. They are about 1.25 inches long, on Sterling silver wire with SS French ear wires.


text:
Q: JOIN / UNION SELECT all rows from two tables with different number of columns I am trying to join or union the results of two differently structured tables, order them by a their common pubdate column, but get an error message:

The used SELECT statements have a different number of columns

SELECT * FROM news WHERE published='1' AND image!='' AND featured='1'
JOIN
SELECT * FROM videos WHERE published='1'
ORDER BY pubdate DESC

How can I edit my query so that I can run my fetch array and retrieve the corresponding rows afterwards (the rows to be fetched is then decided on another common row that both tables share)?

A: Since you not provided sample data, we can't suggest you correct way what and how to use, but I noticed that:
With JOIN you have incorrect syntax. Should be like:
SELECT *
FROM tbl1 t1
INNER JOIN tbl2 t2 ON t1.Id = t2.Id

If you want to use UNION - order of columns and number of columns should match in both tables, so you have to provide column names in both tables, in following:
SELECT Col1, Col2, Coln
FROM tbl1

UNION

SELECT Col1, Col2, Coln
FROM tbl2

A: You can UNION ALL tables with a different number of columns by adding the missing columns in the select list. I mean, suppose you have:
SQL> create table one ( c1 integer , c2 integer, c3 integer ) ;
SQL> create table two ( c1 integer , c2 integer ) ;

The following UNION ALL won't work:
SQL> select * from one union all select * from two ;
[mysqld-5.5.27]The used SELECT statements have a different number of columns

But this one is ok:
SQL> select * from one union all select *, null from two ;

Note we did add NULL for the missing (c3) column on table two. You can add whatever you want...

redpajama_set_name: RedPajamaStackExchange


Description: with thousands of game pitches being made every year, its important to consider the process and decision-making behind publishers and what bests position a game for a publishing offer. From the first email to the pitch deck to the publishing ask, every step of a publishing conversation is important to craft and consider. With real examples of developer pitches at their best (and worst), meetings that have gone wonderfully right (and terribly wrong), this talk aims to unpack the details on game evaluation and how developers can best ready themselves for an amazing publishing conversation.
Targeted public: independent game developers and teams looking to find insight into publishers and investors, getting a real sense of the publishing process and how they can best cater their game pitch to publishers.
Takeaways: a strong understanding of the inner workings of a publisher for developers looking to align with a publisher, investor, or other group to make their game successful.


text:
National security overview
Intelligence Activities Targeting Finland and Finns
Threats to critical infrastructure
Dual-use items and WMD
Supo on social media
Security Clearances
Why are security clearance vettings done
What kind of security clearance vetting does Supo perform
Are you subject to security clearance vetting
Your rights in security clearance vetting
What affects security clearance vetting
The outcome and integrity monitoring
Are you requesting a vetting
Applying for security clearance vetting client status
Organisations responsibilities and obligations
Processing times and fees
Facility security clearance
Requesting facility security clearance
Conducting facility security clearance
Frequently Asked Questions on security clearance vetting
Electronic transaction service
Instructions for requesting a security clearance
Instructions for security clearance vetting subjects
Security clearance register
What Supo does
Intelligence serves the national leadership of Finland
Intelligence legislation
Regulatory control
Counterintelligence
Counterintelligence combats unlawful intelligence operations
Targets of espionage
Cyber espionage
APT operations
Counterproliferation
Supo combats terrorism through intelligence
Terrorist threat assessment
Counterterrorism targets
Radical Islamist terrorism
Isil and Al Qaeda
Extreme right-wing terrorism
Far-right ideology
About Supo
Supo in figures
Working for Supo
Supo's predecessors
Document publicity
Select language Suomi
Select language Svenska
Supo
APT is a toolbox for cyber spies
Cyber espionage operations are often named with the abbreviation APT, together with a number combination. The abbreviation became known in Finland in connection with the APT31 cyber espionage operation against the parliament. Supo compiled some questions and answers concerning APT operations.
In order to intrude into an information system, an individual or entity carrying out a cyber espionage operation needs some tools. Information is sought and copied from the IT system and eventually it is transferred out of the system without anybody noticing.
Connections made to the target often leave a trace. In order to prevent the state behind the operation from being revealed, the individual or entity conducting the operation also needs network infrastructure for covering up the traces. Network traffic may be routed via multiple countries and harmless looking IP addresses so that the operation will not immediately be linked with the perpetrating state.
The abbreviation APT is used to describe such cyber espionage operations. It is not a group consisting of individuals, for example, but a group of technical traces.
Information security community and security authorities are able to identify cyber operations connected with each other with the help of the traces left by the used methods, software tools and network infrastructure. Identified operations may be named in public. APT identifiers often give very clear indications of the state behind the cyber espionage operation and, mostly, also of the intelligence service.
What does the abbreviation stand for?
APT stands for Advanced Persistent Threat.
The notion "APT" was adopted in a time when state-run cyber espionage operations aimed at gaining access to the target and staying there as soon as possible without anyone noticing. Software vulnerabilities of the targeted systems were exploited in the cyber espionage operations.
The operations aim at hiding a malicious code into the targeted system. The code used for cyber espionage operations was very advanced.
Nowadays, "target-oriented" would be a more descriptive term than "advanced". The aim of some operations is still to gain long-term access to the target and to operate without being noticed, whereas others attract attention due to the rudimentary methods and painstaking efforts. It is therefore likely that the aim of such operations is more strongly related to communication than to information gathering.
Cybercrime inspired by financial motives will settle for any vulnerable target that the criminals may exploit in order to achieve financial gain. In cyberespionage, the situation is different. The aim of the operation is to gain access exactly to the specific target. It is therefore in the interests of the perpetrator to try various methods in a persistent manner until a well-functioning one is found.
Cyber espionage is activity that threatens national security. The aim is to gather such information on the target country that restricts its international margin of manoeuvre or affects its status in the global competition.
How are APT operations named?
Each APT has been named by the entity having publicly identified the operation, that is, usually an information security company. Some APTs have many different names because various companies have named them based on their own data. The connection between different APT operations might have been found only at a later stage.
Often the name consists of the abbreviation APT and number but that is not always the case. For example, the operation executed by Russian military intelligence GRU, which was named as APT28, is also known as Sofacy.
Is APT a group of hackers?
No. APT is part of controlled, systematic state-run cyberespionage.
Is APT a malware?
No. Malicious code sent to the target may be used in cyber espionage operations but it is also possible not to use any detectable code. An operation can also be carried out over the Internet by abusing legitimate software installed on the target system.
Finnish Security and Intelligence Service

redpajama_set_name: RedPajamaCommonCrawl


We moved in with a local Muslim family for a week in a fishing village in Kizimkazi because we wanted to experience authentic African lifestyle.
We camouflaged ourselves with culturally appropriate clothing and we hopped on a speedy dalladalla minivan to Kizimkazi.
After two hours of driving, our Dalladalla driver dropped us on a small road near a small village.
The mother of the family Aisha came to greet us and we walked with her to her home, where we will be staying for one week.
The house is a very modest one, made from stone and brick.
There is a chicken in the living room.
There are only two doors in this house, one for the entrance and one for our room. For the rest of the doorways there are only curtains.
Wind passes through the house and gently flows the curtains. There is some space between the walls and ceiling so the wind flows through the house and keeps a constant pleasant temperature.
Aisha's husband also lives here, who is a fisherman, and her mother and four children. The family doesn't speak English.
For a toilet there is a hole in the ground and for showers there is a big bucket of water. We were a bit shy to go to the toilet with just a curtain for a door.
For food we have gotten rice, potatoes and bananas. Everything is eaten by hands, which is pretty damn difficult (especially rice). Perhaps we will master this in a week!
All of the villagers are curious and come to greet us happily. Children stare, smile and laugh. One small little girl was so scared that she burst into tears.
On our arrival we got quite an insane surprise!
We were able to take part in the Kizimkazi village community's large delightful Zanzibar wedding party.
We would never have believed that these ladies can shake their booties like this! We danced till our legs were aching in the centre of the village with all the happy African ladies and tried to sing along local folk music.
This is real life in Zanzibar!
ORiginal text can be found IN IKILOMALLA BLOG.
PHOTOS AND VIDEO BY IKILOMALLA.


The Balsells Graduate Fellowship was created to help Catalan students with excellent academic records and the potential to outstanding contributions to the engineering profession. It has a total value of approximately $58,000 which includes all registration fees and tuition, health insurance, and a monthly stipend of $2,000. The fellowship also provides $1,500 to cover travel expenses.
You may apply for a Balsells Graduate Fellowship if you have Spanish (or another European Union) citizenship, have legally resided (registered to vote) in Catalonia for at least 12 months, fluently speak and write English, Catalan and Spanish, and have received or will receive a 4-year (Bachelor's) or 5-year (superior) degree in Engineering or related field from a recognized Catalan university. You must have received your degree within the last six years or plan to graduate by the end of summer of the year you are applying.
Original (hard copy) or official electronic version submitted directly from your school to UCI in English (or Original in Catalan or Spanish accompanied with an official English translation) academic transcript from the University you attended. Note that not all departments accept electronic transcripts. A transcript that includes the most recent (or final) overall GPA on the scale of 10 is preferred.
IMPORTANT: Contact the Balsells program at balsells@uci.edu several weeks before you submit your application so that you can receive proper advice regarding your specific situation.
It is recommended that the TOEFL (or IELST) and GRE exams be taken in November or December at the latest. Some programs have deadlines as early as December 15 (see DEADLINES below). For further details on admission requirements see Applying to UCI.
Notify the Balsells Program at balsells@uci.edu immediately after submitting your electronic application.
It is very important that all your supporting documents listed above be received by the department you are applying to at UCI no later than the posted DEADLINES for Fall Admission. These deadlines vary by program. In order to be able to apply for the Balsells Fellowship, UCI must receive all of your supplementary documents (TOEFL, GRE, transcripts, letters) no later than February 1 (or earlier if required by the program you are applying to). You will be notified of admission in March.
Step 2: The recipients of the graduate Balsells Fellowship will be chosen from among those Catalan students admitted into UC Irvine's School of Engineering or the Donald Bren School of Information and Computer Sciences. Once you have received notification that you have been admitted, you will be asked to submit a two page PDF document to balsells@uci.edu. The first page of this document is a description of how you expect to contribute to the scientific or technological development of Catalonia after your complete your studies at UC Irvine. The second page is an official certification of residence in Catalonia (certificat d'empadronament) verifying that you have been a resident of Catalonia for at least 12 months.
All Balsells fellowship awards are normally announced in May.


text:
Vienna Gödel Lecture 2014: Erik Demaine
The "Vienna Gödel Lecture of the Faculty of Informatics 2014" will be held on June 4th, 2014 by Erik Demaine from the Massachusetts Institute of Technology. He became with 20 years the youngest professor of computer science.
Algorithms Meet Art, Puzzles, and Magic
Already in his childhood Erik Demaine designed and made puzzles together with his father, and distributed them as the Erik and Dad Puzzle Company to toy stores across Canada. So began the journey into the interactions between algorithms and the arts. More and more, Erik Demaine and his father find that their mathematical research and artistic projects converge, with the artistic side inspiring the mathematical side and vice versa.
Mathematics itself is an art form, and through other media such as sculpture, puzzles, and magic, the beauty of mathematics can be brought to a wider audience. These artistic endeavors also provide us with deeper insights into the underlying mathematics, by providing physical realizations of objects under consideration, by pointing to interesting special cases and directions to explore, and by suggesting new problems to solve.
This talk will give several examples in each category, from how the first font design led to building transforming robots, to how studying curved creases in origami led to sculptures at MoMA. The audience will be expected to participate in some live magic demonstrations.
17:30 Welcome
Johannes Fröhlich, Vice Rector for Research, TU Vienna
Gerald Steinhardt, Dean of the Faculty of Informatics, TU Vienna
17:45 Algorithms Meet Art, Puzzles, and Magic
Erik Demaine, Massachusetts Institute of Technology, USA
Moderation: Stefan Szeider, Institute of Information Systems, TU Vienna
The Vienna Gödel Lectures
The Faculty of Informatics at the Vienna University of Technology established, starting with a talk by Donald E. Knuth in 2013, the annual "Vienna Gödel Lectures of the Faculty of Informatics". The aim of this series is to render Vienna attractive to world-renowned computer scientists, raising its profile as an academic hotspot. Furthermore, this series emphasizes the importance of computer science and its significant contribution to explaining and shaping the world in which we live today.
The lecture series is named after the famous mathematician and logician Kurt Gödel, who accomplished essential parts of his scientific work while in Vienna.
Keine Anmeldung notwendig! Der Livestream wird direkt auf der Youtube-Startseite der TU Wien zu erreichen sein: www.youtube.com/tuwienprmedia
Wed, June 4, 2014
17:30 –19:30, s.t.
Prof. Erik Demaine
TU Wien, Campus Gußhaus, EI 7
Vienna Gödel Lectures


The Innominates and Pubic Symphysis course has a lecture on the functional anatomy pearls for the innominates and the pubic symphysis. Then, the primary focus of the course is on the lab demonstrations of the dysfunctions of the innominates and the pubic symphysis. The core manual medicine treatment modalities covered in this course are Muscle Energy, HVLA, the Still Technique, and Soft Tissue Techniques.
Understand the functional anatomy of the innominates and the pubic symphysis.
Review how to diagnose and treat the somatic dysfunctions of the innominates and the pubic symphysis.
Understand how to apply HVLA, Muscle Energy, Soft Tissue Techniques, and the Still technique to the tissues of the innominates and the pubic symphysis.
The Innominates and Pubic Symphysis Course: 2.5 Hours. This includes watching the video course, practicing the technique, filling out an evaluation and taking the test.


text:
Jevgenia Romanjoeta (Russisch: Евгения Сергеевна Романюта) (Toela, 22 januari 1988) is een wielrenner uit Rusland.

In 2011 werd Romanjoeta Europees kampioen baanwielrennen op het onderdeel puntenkoers, een jaar later behaalde ze de zilveren medaille.

In 2012 reed Romanjoeta op de Olympische Zomerspelen in Londen op het onderdeel omnium op de baan.

In 2013 reed Romanjoeta met het Russische team op de Europese kampioenschappen op het onderdeel achtervolging naar een bronzen medaille, en in 2014 naar een zilveren medaille. Ook in 2015 wist ze deze prestatie op dit onderdeel te evenaren.

Russisch baanwielrenner
Russisch olympisch deelnemer

redpajama_set_name: RedPajamaWikipedia


I hope you all had an awesome weekend! Today's look is a fun and interesting one, since we have the mix of colors and patterns, but in a way that's more subtle. If you remember a few weeks ago, I recorded a video, How to Pattern Mix Like a Pro, in which I explained some of the methods you see demonstrated in this pairing. First, you'll notice that I selected my upper body to feature the largest and most vibrant print and the shoes to feature the smallest and darkest. The location or placement of the size of the print will vary depending on your body shape and where you want the pattern to stand out most. For me, since I'm a pear shape, I want the volume to be placed up top, to balance out my hips, which is why I opted for this bomber.
Another strategy you'll notice that I mentioned in the video, was the colors used for both patterns. I mentioned in the video that if you're not certain if a print goes together, select patterns that feature the same or similar color scheme, to create a nice blended look. That's exactly what I did here. Both pieces have blue, white, and a deep red, which creates a cohesive and blended look, one that doesn't clash.
Below is a very similar look I created, regardless of your body shape. Although I mentioned above that the location or placement of the prints will vary depending on your body shape, if you happen to like this very look, I'm giving you an idea how you can still pull it off, regardless of your shape or silhouette. Remember, in fashion, there are generally exceptions to the "rules", it's just a matter of selecting pieces that can help bring the look together in a way that's flattering to successfully pull it off!
If you have larger hips, i.e. a pear or hourglass shape, you can wear the look as I'm wearing it above with a dark wash skinny jean. Although the leg is slim and can make the hips appear wider, the fact that it's in a dark wash with minimal fading will help counteract that. However, there is another style that would work and that's a flared leg in a dark wash.
If you have a larger bust or midsection, such as an apple or inverted triangle shape, a light wash bootcut with a substantial amount of fading, will help in preventing the bust or midsection from appearing larger, due to the volume of the bomber and print. The width of the bootcut will help balance out the width up top and the lighter denim will help add some visual weight to your lower body, since white and lighter colors help reflect light.
I hope this post inspired you to play around with some paisley and polka dotted pieces you may have in your wardrobe!
PS: The 7 for all mankind jeans seen in the set I created above can be found at an outlet store or search your local Marshalls, Tjmaxx, or Burlington Coat Factory for a much more cheaper price!


Welcome Ametista! :bearhug: I'm happy you found this forum.
Great to have you with us here Ametista. Welcome to the hoax family on this forum.
Hi Ametista, and welcome to the hoax family!
Enjoy the journey, cause it's a beautiful one!
Welcome i hope you enjoy it here.


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What Type of Pots to Put Hibiscus Plants In?
By Joanne Marie
Garden Urns & Planters
The Lowest Temperature for the Tropical Plant Bougainvillea
Can I Make a Planter Out of a Cauldron?
Planters for Tall Cactuses
How to Re-Pot Jasmine
For large, showy flowers, few plants surpass the tropical hibiscus (Hibiscus rosa-sinensis), a frost-tender plant that does well as a potted specimen. The hibiscus is available in dozens of cultivars, with flowers that can be single or double and come in a wide array of single or mixed colors. Growing this impressive plant in a container allows it to overwinter indoors in cold-winter areas, and choosing the best type of container can help ensure its health and long-term survival.
Drainage Is Crucial
It's critical for any potted plant to have good drainage, so that water can drain freely from the pot. This helps prevent overwatering that can lead to root rot and other fungal diseases. When choosing a pot for a hibiscus plant, it's best to pick one that has several drainage holes. If your pot has a single hole and it's plastic or another material unlikely to crack, you can use a hand drill or electric tool to add additional holes, helping the plant's soil drain fully after each watering.
Although the size of the best pot depends to some degree on the size of the hibiscus plant, the hibiscus tends to produce a wide root ball rather than a deep one. For this reason, use a pot that's at least 10 inches wide for a young, nursery-grown specimen. If your plant is already large and you want to repot it from a nursery pot into a more decorative container, choose one that's at least a few inches larger in diameter that the current pot to allow for new growth.
Hibiscus plants are sensitive to overheating, especially if kept outdoors in summer, and can suffer when their roots remain dry for any period of time. A heavy pot made of clay provides good stability and is also unlikely to overheat, because clay is porous and releases hot air. You can also use a plastic pot, but avoid a black or dark-colored pot, because it can heat up in the sun and cause root burn. You could place a dark-colored plastic pot inside a larger clay pot, to prevent overheating and also keep the plant stable, but always separate the pots for a few minutes after watering, to let the plant's soil drain well.
Other Needs
The tropical hibiscus, also called the Chinese hibiscus, can grow outdoors year-round in U.S. Department of Agriculture plant hardiness zones 9 through 11. When container-grown, it does well indoors during winter in colder regions. The plant prefers a sunny indoor spot and thrives near a south- or west-facing window. If you keep the plant outdoors during warm months, it can take full sun, but move it into bright outdoor light gradually, adding an hour or two each day, to prevent leaf scorch. The hibiscus needs even moisture and prefers a deep watering that reaches all the roots, repeated whenever the top few inches of soil feel dry to the touch.
New Orleans Chapter of the American Hibiscus Society: Hibiscus in Pots -- Container Growing
Louisiana State University AgCenter: Tropical Hibiscus
Hidden Valley Hibiscus: Potting and Planting Hibiscus
Missouri Botanical Garden: Hibiscus Rosa-Sinensis
Joanne Marie began writing professionally in 1981. Her work has appeared in health, medical and scientific publications such as Endocrinology and Journal of Cell Biology. She has also published in hobbyist offerings such as The Hobstarand The Bagpiper. Marie is a certified master gardener and has a Ph.D. in anatomy from Temple University School of Medicine.
How to Choose Pots for Hibiscus Trees
Do I Have to Have a Drainage Hole in Large Indoor Planters?
How to Repot Hibiscus
Repotting Chamaedorea Elegans
How to Repot Ficus Benjamina
Care & Maintenance of Tropical Hibiscus
How to Grow a Standard Hibiscus
How to Maintain an Indoor Plant
How to Ensure Adequate Drainage When Using Flowerpots
1 How to Choose Pots for Hibiscus Trees
2 Do I Have to Have a Drainage Hole in Large Indoor Planters?
3 How to Repot Hibiscus
4 Repotting Chamaedorea Elegans


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Clustered around the heart of the hotel, all 31 Courtyard Suites provide direct and easy access to the Main Building and many of Raffles' signature facilities. Indulge at Raffles Spa, shop at Raffles Arcade, and then come back to your own personal oasis. Step from your parlour to the verandah to admire lush gardens lined with leafy ferns – for a sense of serenity, sheltered from the tropical heat. A king bed or two queen beds await you in your beautiful bedroom.
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July is giving way to August, and the very first of the northbound thru-hikers are answering the siren song of Mount Katahdin. A huge round of applause for these brand-spanking-new thru-hikers!
Whether you're going northbound, southbound, or flip-flopping, we want to feature the photo of you crossing the finish line! This week contains photos submitted by hikers who have finished by July 22, 2018.
Be sure to email your photos to [email protected] and include your trail name and completion date!
would definitely jump out and compliment the rich dark wood furniture appropriate for oriental decorating.
Awesome photos that make me smile. Well done hikers!


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HEVC stands for "High Efficiency Video Coding" and it is a video compression standard developed by the Joint Collaborative Team on Video Coding; it offers about double the data compression ratio at the same level of video quality (or substantially improved video quality at the same bit rate) of the widely used AVC (H.264 or MPEG-4 Part 10). It also supports resolutions up to 8192×4320, including 8K UHD.
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Site Coming Soon
Eleanor P. (Gurski) Lombard
Eleanor P. (Gurski) Lombard, 86, of Shenandoah Heights, passed away peacefully Monday at Shenandoah Senior Living Community.
Born in Shenandoah, June 26, 1928, she was a daughter of the late Stanley and Julia (Rudalavage) Gurski.
Eleanor was a member of Divine Mercy Parish, Shenandoah, and a former member of Our Lady of Mount Carmel Roman Catholic Church, Shenandoah. She was also a member of the ILGWU.
Mrs. Lombard worked in the local garment industry. She was last employed at Shenandoah Manor in the dietary department.
She was the last surviving member of her immediate family.
Preceding her in death, in addition to her parents, were her husband, Sam A. Lombard, on Dec. 15, 1993, and a daughter, Sharon Lombard Misunas, on Nov. 8, 2001.
Surviving are a son, James S. Lombard and his wife, Gina, Shenandoah Heights; a daughter, Rose Marie McHugh and her husband, John, Weatherly; six grandchildren, 10 great-grandchildren; nieces and nephews.
Private services and interment will be held at the convenience of the family. Walu-kiewicz-Oravitz Fell Funeral, 132 S. Jardin St., Shenandoah, is in charge of the arrangements.
Eleanor P. (Gurski) Lombard Has 3 Condolences Posted:
Kendall Baab says:
Jimmy,
I am sorry to hear about the loss of your Mother. My thoughts and prayers are with you and your family.
Kendall Baab
Vicky Guydish says:
My sincerest sympathy on the loss of your Mom. Sending prayers for you and your family.
Vicky Guydish
Marianne and Larry Nelson says:
So sorry to hear about your Mom, please know that we are thinking of you, your brother and your families at this sad time.
Marianne and Larry Nelson
© 2020 Walukiewicz-Oravitz Fell Funeral Home. All rights reserved.


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L'ultimo Abenzerraggio (Le Dernier Abencérage) est un opéra en quatre actes de Felipe Pedrell i Sabaté.

Présentation
Inspiré par la nouvelle Les Aventures du dernier Abencerage de Chateaubriand, l'opéra est composé en 1867 par le compositeur Felipe Pedrell, qui effectue plusieurs versions jusqu'à la définitive de 1889. L'opéra est écrit en italien par Francesc Fors de Casamajor et il est créé au Grand théâtre du Liceu de Barcelone le 14 avril 1874.

Bien qu'il n'ait fait l'objet que de cinq représentations, il reçoit un accueil favorable tant du public que de la critique.

La partition est publiée en 1874 par l'éditeur Andrés Vidal y Roger de Barcelone, et dédiée à la cantatrice Ebe Trèves, interprète lors de la création de l'opéra, pour sa partie chantée. Il en est de même pour Giuseppina Borsi de Giuli.

Interprètes

Ce sont les cantatrices Giuseppina Borsi de Giuli (fille de la soprano Teresa de Giuli Borsi) et Ebe Trèves (nom réel Anna Giustina Ebe), ainsi que les chanteurs Carlo Carpi, Antonio Vidal et Francesc Viñals qui interprètent l'œuvre, dirigée par le chef d'orchestre Eusebi Dalmau.

Références

Liens externes

Opéra créé à Barcelone
Opéra en italien
Opéra des années 1870


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