text:
\section{Introduction}

The lithium-like \ion{O}{6}\ ion is an important tool for studying hot gas in interstellar space, because emission via its 1031.93 and 1037.62 \AA\ resonance lines is the dominant cooling mechanism for gas at temperatures of a few times $10^5$ K \citep{Gnat:Sternberg:07}.  Recent \ion{O}{6}\ absorption-line surveys \citep{Savage:03, Bowen:08} reveal that, within our Galaxy, the \ion{O}{6} -bearing gas has an exponential scale height of 3.2 kpc at negative latitudes and 4.6 kpc at positive latitudes.  The gas is clumpy: spectra of nearly two dozen stars in the Large and Small Magellanic Clouds reveal significant variations in the \ion{O}{6}\ column density of Galactic halo gas over angular scales as small as $3\farcm5$ \citep{Howk:02}.

Closer to the plane, \citet{Bowen:08} find that the average volume density of \ion{O}{6}\ towards stars in the Galactic disk, $n = N($\ion{O}{6}$)/d$, exhibits a dispersion of about 0.26 dex, regardless of the distance to the target stars.  They conclude that the \ion{O}{6}\ does not arise in randomly distributed clouds of a uniform size and density, but is instead distributed among regions with a broad range of column densities, with smaller clouds more common and larger clouds less so.  They envision a turbulent, multiphase medium churned by shock-heated gas from multiple supernova explosions.

\defcitealias{Otte:06}{Paper~I}
\defcitealias{Dixon:06}{Paper~II}

We present the latest results from a survey of diffuse \ion{O}{6}\ emission from the interstellar medium (ISM) conducted with the {\it Far Ultraviolet Spectroscopic Explorer (FUSE)}.\/  \citet[hereinafter Paper~I]{Otte:06} and \citet*[Paper~II]{Dixon:06} discuss observations obtained from launch through 2003 July 25 and 2004 December 31, respectively.
In these papers, \ion{O}{6}\ emission at 3$\sigma$\ significance is detected along 29 lines of sight.  Measured intensities range from 1.8 to 9.1 kLU, with a median of 3.3 kLU.  An additional 35 sight lines provide upper limits of 2.0 kLU or less.  (One line unit, or photon cm$^{-2}$ s$^{-1}$ sr$^{-1}$, corresponds to $1.9 \times 10^{-11}$ erg cm$^{-2}$ s$^{-1}$ sr$^{-1}$ at 1032 \AA.)  By combining emission and absorption measurements through the same \ion{O}{6} -bearing regions, the authors find evidence for two flavors of \ion{O}{6} -emitting gas: relatively narrow, high-density conductive interfaces in the local ISM and more extended, low-density regions in HVCs.

In this paper, we present data obtained between 2005 January 1 and 2007 July 6, along with two older observations that were missed in the earlier papers.  In \S \ref{sec_observations}, we describe the {\it FUSE}\/ instrument, our criteria for selecting sight lines for study, and our data-reduction and analysis techniques.  In \S \ref{sec_discussion}, we derive the physical parameters of the emitting gas and discuss its location along the line of sight.  We present our conclusions in \S \ref{sec_conclusions}.  Because the {\it FUSE}\/ pointing system failed in July of 2007, these observations represent the final installment of our survey.

\section{Observations, Data Reduction, and Analysis} \label{sec_observations}

{\it FUSE}\/ consists of four coaligned spectrographs. Two employ Al+LiF optical coatings and record spectra over the wavelength range 990--1187 \AA, while the other two use SiC coatings, which provide reflectivity to wavelengths below the Lyman limit. The four channels overlap between 990 and 1070 \AA.  Each channel possesses three apertures that simultaneously sample different parts of the sky. The low-resolution (LWRS) aperture is 30\arcsec\ $\times$ 30\arcsec\ in size. The medium-resolution (MDRS) aperture is 4\arcsec\ $\times$ 20\arcsec\ and lies about $3\farcm5$ from the LWRS aperture. The 1.25\arcsec\ $\times$ 20\arcsec\ high-resolution (HIRS) aperture lies midway between the MDRS and LWRS apertures. A fourth location, the reference point (RFPT), is offset from the HIRS aperture by about 1\arcmin. When a star is placed at the reference point, all three apertures sample the background sky.  For a complete description of {\it FUSE}, see \citet{Moos:00} and \citet{Sahnow:00}.

To identify background observations for this study, we searched the Multimission Archive at Space Telescope (MAST) for {\it FUSE}\/ data obtained after 2005 January 1 falling in one of three categories: programs S405, S505, S605, S705, and S905, which consist of background observations obtained during spacecraft thermalization periods; MDRS, HIRS, and RFPT observations of point sources, for which the LWRS aperture should sample only background sky; and targets whose names include the strings ``BKG'' or ``SKY.''  To find older observations that may have been missed in our previous studies, we searched the entire archive for target names that include the strings ``OFF,'' ``SKY,'' or ``WIND.''

We exclude from our sample known supernova remnants, nebulae, and point-source targets in either of the Magellanic Clouds.  Data from programs E124, G052, and G938 will be published elsewhere.  Because its sensitivity at 1032 \AA\ is more than twice that of any other channel, we consider only data from the LiF 1A channel.  We use only data obtained in time-tag mode, which preserves arrival time and pulse-height information for each photon event.  To avoid contamination by geocoronal emission \citep*{Shelton:07}, we use only data obtained during orbital night.  Individual exposures with less than 10 s of night exposure time are excluded from the survey, as are combined data sets with less than 1500 s of night exposure time or with significant continuum flux.  Our final sample consists of data obtained along 120 lines of sight.

The data were reduced using an implementation of CalFUSE v3.2, the latest version of the {\it FUSE}\/ data-reduction software package \citep{Dixon:07}, optimized for faint, diffuse emission.  Details are given in \citetalias{Dixon:06}, but we highlight a few points here:  the program operates on one exposure at a time, producing a flux- and wavelength-calibrated spectrum from each.  Background subtraction is turned off.  Zero-point errors in the wavelength scale are corrected by fitting a synthetic emission feature to the Ly $\beta$ airglow line.  The spectra from individual exposures are then shifted to a heliocentric wavelength scale and combined.

We use an automated routine to search each combined spectrum for statistically significant emission near 1032 \AA.  When we find it, we fit the line with a model emission feature using the non-linear curve-fitting program {\small SPECFIT}\ \citep{Kriss:94}.  The model consists of a top-hat shaped function 106 km s$^{-1}$\ in width, representing the LWRS aperture, convolved with a Gaussian, representing the instrument line-spread function ($\sim$ 25 km s$^{-1}$ ) convolved with the intrinsic emission-line profile.  Free parameters in the fit are the level and slope of the background (assumed linear) and the amplitude, central wavelength, and FWHM of the Gaussian.

While we use the same line identification and fitting algorithms described in \citetalias{Dixon:06}, one change in our technique is worth noting:  Because our count rates are low, we bin the spectra to raise the counts per bin into the regime where Gaussian statistics apply.  For most spectra, we bin by 14 pixels or 53 km s$^{-1}$, a value chosen so that that two binned pixels just span a diffuse emission feature.  If the continuum averages more than 1.5 counts per pixel, we take advantage of the higher signal-to-noise ratio and bin by only 8 pixels.  Because narrow emission features may be undersampled by 14-pixel binning, in \citetalias{Dixon:06} we lowered the threshold for 8-pixel binning to 0.5 counts per bin for spectra containing features with FWHM $< 100$ km s$^{-1}$.  In this paper, we use 14-pixel binning for all faint continua, regardless of the line width.  Implications of this change are discussed below.

Our automated routine flags 32 spectra as having statistically significant \ion{O}{6}\ emission; i.e., the intensity of a putative emission feature is greater than 3 times the uncertainty in the local continuum.  For only 13 of these spectra do model fits return line intensities with $I/\sigma(I) \geq 3$.  We refer to these features as 3$\sigma$\ detections.  Lines with $I/\sigma(I) < 3$ are referred to as 2$\sigma$\ detections.  The best-fit parameters for both sets of \ion{O}{6}\ features are presented in Table \ref{tab_detections}, and plots of the spectra and best-fit models are presented in Figures \ref{fig_3sigma} and \ref{fig_2sigma}.  The asymmetric shapes of the narrowest model emission features are artifacts of our sparse sampling of the model lines.

Measured intensities range from 2.8 to 10.5 kLU, with a median of 4.0 kLU.  Five of our 3$\sigma$\ detections have local standard of rest velocities $|v_{\rm LSR}| > 60$ km s$^{-1}$, while the rest have $|v_{\rm LSR}| < 35$ km s$^{-1}$.  Four sight lines have FWHM values $< 25$ km s$^{-1}$, indicating that their \ion{O}{6}\ emission does not fill the LWRS aperture.  For these sight lines, the surface brightness of the emitting region is underestimated and the velocity uncertain, as discussed in \citetalias{Dixon:06}.
For the non-detection sight lines, we compute 3$\sigma$\ upper limits to the intensity of an \ion{O}{6}\ emission feature using the mean background intensity between 1030 and 1035 \AA\ and assuming a line width of 28 pixels (106 km s$^{-1}$).   Upper limits for 15 sight lines with $I(\lambda 1032) \leq 2$ kLU are given in Table \ref{tab_limits}.

Four of our sight lines are previously published, but we include them here because additional data are now available.  The original 26 ks observation of sight line B12901 is analyzed by \citet{Shelton:03} and in \citetalias{Dixon:06}.  Recently, this line of sight was re-observed as target U10635, increasing the total exposure time to 40 ks.  For this line of sight, an upper limit of 1.5 kLU is reported in \citetalias{Dixon:06} (see their Table 6); our new upper limit is 1.2 kLU.  Similarly, sight line C15301 was re-observed as target U10631, increasing the total exposure time from 93 to 102 ks.  Our results (Table \ref{tab_detections}) are consistent with those of \citet{Shelton:07}, who analyze the original C15301 data.  A 5.2 ks observation of sight line S40577 was analyzed in \citetalias{Dixon:06}, resulting in an upper limit of 3.6 kLU (see their Table 4).  The total exposure time is now 24 ks, and our upper limit has fallen to 1.7 kLU.

Finally, a second observation of sight line S40590 has increased its exposure time from 10.8 to 15.2 ks.  The measured flux is unchanged from that reported in \citetalias{Dixon:06}, but the best-fit radial velocity has risen from $-49$ to $-18$ km s$^{-1}$.  Part of this change may be attributed to the fact that, because the feature is so narrow, we binned the spectrum by 8 pixels in \citetalias{Dixon:06}, while we bin it by 14 pixels for this paper.  Binning the current spectrum by 8 pixels yields a best-fit velocity of $-29 \pm 17$ km s$^{-1}$.  The larger problem is that the emission feature, with FWHM = 9 km s$^{-1}$, is unresolved, suggesting that the emitting region is smaller than the LWRS aperture.  The uncertainty of its position within the aperture adds a systematic velocity uncertainty of about 50 km s$^{-1}$.

\section{Discussion} \label{sec_discussion}

\subsection{Probing the Southern Galactic Sky} \label{sec_map}

Examination of Tables \ref{tab_detections} and \ref{tab_limits} reveals that most of the \ion{O}{6}\ detection sight lines in our sample lie in the region of the southern Galactic sky between $l$ = 180\arcdeg\ and 360\arcdeg, while most of our upper limits lie in the region of the northern Galactic sky between $l$ = 0\arcdeg\ and 180\arcdeg.  The prominence of these two quadrants in the {\it FUSE}\/ target list is discussed in \citetalias{Otte:06} and reflects observational constraints that reduced target availability in the orbit plane.  The dearth of \ion{O}{6}\ detections among our northern sight lines may reflect their generally lower galactic latitudes, which are more likely to suffer significant extinction.  Happily, the southern quadrant between $l$ = 180\arcdeg\ and 360\arcdeg\ is now reasonably well sampled in \ion{O}{6}\ emission, and we focus our attention there.

Figure \ref{fig_map} presents a map of the southern Galactic sky centered on the Magellanic Clouds.  The background image is an \ion{H}{1}\ map based on 21 cm emission measurements.  Velocities are color-coded, with purple/blue representing negative velocities and orange/red representing positive velocities.  Overplotted are large circles representing sight lines with significant high-velocity \ion{O}{6}\ absorption from the surveys of \citet{Sembach:03} and Wakker (in preparation).  Their colors indicate the velocity of the absorbing gas using the same color scale as the \ion{H}{1}\ emission.  Small open circles indicate null detections.  The large squares represent 3$\sigma$\ \ion{O}{6}\ detections from this survey and that of \citetalias{Dixon:06}, also color-coded by velocity.  Small open squares represent interesting upper limits ($I(\lambda 1032) \leq 2$ kLU) from both this survey and \citetalias{Dixon:06}.  For convenience, the \ion{O}{6}\ detections and limits taken from \citetalias{Dixon:06} are reproduced in Tables \ref{tab_old_detections} and \ref{tab_old_limits}.

Immediately apparent in \fig{fig_map} are the many sight lines exhibiting low-velocity \ion{O}{6}\ emission (green squares).  Their wide distribution, extending to low galactic latitudes, suggests that they trace a larger structure (\S \ref{sec_compare}).  Among the low-velocity sight lines are two that also exhibit \ion{O}{6}\ absorption (Fairall~9 and NGC~625), from which we can derive the physical parameters of the \ion{O}{6} -bearing gas (\S \ref{sec_parameters}).  Finally, the three sight lines showing high-velocity \ion{O}{6}\ emission (S70504, S90513, and I20505) allow us to probe the Magellanic System (\S \ref{sec_magellanic}).

\subsection{Comparing Low and High Latitudes} \label{sec_compare}

In \citetalias{Dixon:06}, we found evidence for two distinct flavors of \ion{O}{6} -emitting gas: relatively narrow (0.1 pc), high-density (0.1 cm$^{-3}$) conductive interfaces in the local ISM and more extended (100 pc), low-density (0.01 cm$^{-3}$) regions in high-velocity clouds.  To look for evidence of this dichotomy within our current data set, we plot the measured \ion{O}{6}\ emission line intensity, line width, and velocity for the low-velocity 3$\sigma$\ emission features shown in \fig{fig_map} as a function of galactic latitude.  The \ion{O}{6}\ intensities are plotted in \fig{fig_intensity}.  Overplotted is the color excess $E($\bv)\ along each line of sight \citep*{Schlegel:98}.  The figure includes a single sight line, S50508, with an \ion{O}{6}\ intensity of 9.1 kLU and a color excess $E($\bv)\ = 1.26 (off scale).  As discussed in \citetalias{Dixon:06}, this sight line probes the outskirts of the Vela supernova remnant (250 pc distant).  As it is not representative of the general ISM, we will not discuss it further.

The other sight lines fall into two groups: those at latitudes $|b| > 30\arcdeg$, which suffer little reddening and whose intensities appear to fall with distance from the plane, and those with $|b| < 30\arcdeg$, which suffer significant reddening.  A color excess of $E($\bv)\ = 0.2 corresponds to an attenuation factor of 14 \citep{Fitzpatrick:99}, so it is unlikely that much of the absorbing material lies between us and the emitting gas.  Either these low-latitude sight lines probe relatively nearby gas, or the extinction is patchy -- or both.

The Gaussian FWHM values are plotted in \fig{fig_fwhm}.  This parameter represents the combined effects of the instrumental line-spread function ($\sim$ 25 km s$^{-1}$) and the intrinsic velocity structure of the \ion{O}{6} -emitting gas.  Though the uncertainties are large, the dichotomy between high- and low-latitude sight lines persists, with generally broad emission features at high latitudes and generally narrow features at low latitudes.  It is striking that all four unresolved emission features (those with FWHM $<$ 25 km s$^{-1}$, indicating that they do not fill the 30\arcsec\ $\times$ 30\arcsec\ LWRS aperture) lie at latitudes $|b| < 30\arcdeg$.  If their emitting regions lie within 1 kpc of the earth, then they have a maximum projected spatial extent of 0.15 pc, similar to the path lengths derived for conductive interfaces in the local ISM \citepalias{Dixon:06}.  At temperatures near $3 \times 10^5$ K, thermal broadening would produce line widths of 40 km s$^{-1}$\ (after convolution with the {\it FUSE}\/ line-spread function), so the broad emission features, more common at high latitudes, sample either turbulent gas or multiple emitting regions spanning a range of velocities.

The LSR velocities are plotted in \fig{fig_velocity}.  Grey bars represent the range of velocities predicted for each sight line by a simple model of Galactic rotation.  Assuming a differentially-rotating halo with a constant velocity of $v = 220$ km s$^{-1}$\ and a distance from the sun to the Galactic center of 8.5 kpc, we compute the expected radial velocity as a function of distance for the first 5 kpc along each line of sight.  The model ignores broadening due to turbulence or any other motion.  While most of the low-latitude sight lines exhibit \ion{O}{6}\ velocities that are generally consistent with our model, most of the high-latitude sight lines do not.  Instead, most are moving away from the Galactic plane at 10--30 km s$^{-1}$.

These trends are consistent with the picture derived in \citetalias{Dixon:06}: that low-latitude sight lines tend to sample relatively small, dense regions in the local ISM, while high-latitude sight lines sample larger, lower-density, more turbulent regions farther from the disk.  In the following two sections, we quantify the physical properties of these high-latitude emitting regions.

\subsection{\ion{O}{6}\ Column Density} \label{sec_absorption}

Figure \ref{fig_map} reveals \ion{O}{6}\ absorption and emission along two pairs of closely-spaced sight lines: toward the galaxies Fairall~9 and NGC~625.  The Fairall~9 sight lines are more closely spaced.  In an effort to observe \ion{O}{6}\ emission corresponding to the high-velocity \ion{O}{6}\ absorption seen in the spectrum of Fairall~9 \citep{Wakker:03}, sight line D02401 was offset from the galaxy by about 1\arcmin.  NGC~625 was observed in the usual way, with the galaxy in the MDRS aperture and the LWRS aperture observing the background sky some $3\farcm5$ distant.

To measure the \ion{O}{6}\ column densities at velocities corresponding to their observed \ion{O}{6}\ emission, we obtained the fully-reduced {\it FUSE}\/ spectra of both galaxies from MAST.  When processing spectra from faint targets, the {\it FUSE}\/ data-reduction pipeline runs CalFUSE (version 3.2.1) on each individual exposure, combines the data from all exposures into a single photon-event list, and extracts one spectrum for the whole observation.  This technique maximizes the fidelity of the two-dimensional scattered-light model that is subtracted from the data.  The resulting spectra are plotted in the top panels of Figs.\ \ref{fig_D02401} and \ref{fig_D04001}.  Both sight lines lie in the direction of the Magellanic Stream, and both spectra show \ion{O}{6}\ absorption extending to high velocities.  Following \citet{Wakker:03}, we choose 100 km s$^{-1}$\ as the dividing line between Galactic and Magellanic absorption.

We approximate an LSR velocity scale by shifting the spectra so that the interstellar \ion{Ar}{1} $\lambda 1048.2$  line falls at its laboratory wavelength, then fit a low-order polynomial to the continuum on either side of the \ion{O}{6}\ absorption.  To account for absorption by molecular hydrogen, we scale the model continuum by a synthetic P(3) $\lambda 1031.2$ absorption spectrum using the column densities, velocities, and line widths of \citet{Richter:01}, \citet{Wakker:06}, and B. P. Wakker (2008, private communication).  H$_2$\ absorption is seen at velocities of $-1$ and 196 km s$^{-1}$\ toward Fairall~9 and 0 and 396 km s$^{-1}$\ toward NGC~625, as shown in the second panel of Figs.\ \ref{fig_D02401} and \ref{fig_D04001}.

We derive \ion{O}{6}\ column densities using the apparent optical depth method \citep{Savage:Sembach:91}, which is applicable when the spectral line to be measured is unsaturated and nearly resolved.  The third panel of Figs.\ \ref{fig_D02401} and \ref{fig_D04001} shows the resulting column density $N_a$(\ion{O}{6}) as a function of velocity.  (Note that $N_a$ is plotted in units of cm$^{-2}$ per velocity bin.)  The resulting column densities for the low-velocity gas ($-110 < v < 100$ km s$^{-1}$) are $\log N = 14.38$ [cm$^{-2}$] toward Fairall~9 and $\log N = 14.50$ toward NGC~625.  Our result for Fairall~9 is identical to that of \citet{Savage:03}, though they do not correct for H$_2$\ absorption in this spectrum.

The fourth panel of Figs.\ \ref{fig_D02401} and \ref{fig_D04001} reproduces the \ion{O}{6}\ emission spectrum for each sight line.  In both cases, the peak of the \ion{O}{6}\ emission lines up nicely with the low-velocity component of the apparent column density $N_a$(\ion{O}{6}).  We can quantify this alignment by computing the average LSR velocity of the Galactic \ion{O}{6}\ absorption ($-110 < v < 100$) using Equation 3 of \citet{Savage:03}.  For Fairall~9, $\bar{v} = 35$ km s$^{-1}$, consistent with the velocity ($16 \pm 21$ km s$^{-1}$) of the emitting gas.  (\citealt{Savage:03} derive $\bar{v} = 24$ km s$^{-1}$\ over the same velocity range.)  For NGC~625, $\bar{v} = 28$ km s$^{-1}$, again consistent with the velocity ($19 \pm 18$ km s$^{-1}$) of the \ion{O}{6}\ emission.

\subsection{Physical Parameters of the High-Latitude Gas} \label{sec_parameters}

Measurements of \ion{O}{6}\ absorption and emission can be combined to provide valuable diagnostics of the \ion{O}{6} -bearing gas.  Because the \ion{O}{6}\ column density is proportional to the density of the gas, while the line intensity is proportional to the density squared, the ratio of intensity to column density is proportional to the electron density in the emitting plasma.

The observed \ion{O}{6} $\lambda$1032 intensity toward Fairall~9 is $3.5 \pm 1.1$ kLU.  We assume that the intrinsic intensity of the \ion{O}{6} $\lambda$1038 emission is half that of the 1032 \AA\ line, as would be expected if the emitting gas were optically thin.  The column density of the low-velocity ($-110 < v < 100$) \ion{O}{6}\ is $\log N = 14.38$.  For an assumed temperature of $2.9 \times 10^5$ K, Equation 5 from \citet{Shull:Slavin:94} yields an electron density $n_{\rm e}=9.5 \times 10^{-3}$ cm$^{-3}$ and a thermal pressure $P/k = 1.92 \, n_{\rm e} \, T = 5300$ K cm$^{-3}$.  The color excess toward Fairall~9 is $E($\bv)\ = 0.025 \citep{Schlegel:98}, which attenuates emission at 1032 \AA\ by $\sim$ 30\% \citep{Fitzpatrick:99}.  If all of that material lies between us and the emitting gas, $n_{\rm e}$ rises to $1.3 \times 10^{-2}$ cm$^{-3}$ and $P/k$ to 7400 K cm$^{-3}$.

To calculate the \ion{O}{6} density and the path length through the emitting gas, we need the oxygen abundance and the fraction of oxygen in O$^{+5}$.  From their sample of low-density ($\langle n_{\rm H} \rangle < 1.0$ cm$^{-3}$) Galactic sight lines longer than 800 pc, \citet{Cartledge:04} derive a mean interstellar O/H ratio of $(4.37 \pm 0.09) \times 10^{-4}$.  For plasmas in collisional ionization equilibrium, the O$^{+5}$ fraction peaks at 21.5\% when the gas temperature is $2.9 \times 10^5$ K \citep{Gnat:Sternberg:07}.  With these values, and assuming that the gas is completely ionized ($n_{\rm e} = 1.2 n_{\rm H}$), we derive an \ion{O}{6} density of $7.4 \times 10^{-7}$ cm$^{-3}$ and a path length through the gas of 100 pc for zero reddening.  If $E($\bv)\ = 0.025, then the \ion{O}{6} density and path length become $1.0 \times 10^{-6}$ cm$^{-3}$ and 75 pc, respectively.

The observed \ion{O}{6} $\lambda$1032 intensity toward NGC~625 is $2.6 \pm 0.8$ kLU and the column density of its low-velocity gas is $\log N$ = 14.50.  From these values, we derive an electron density for the \ion{O}{6} -bearing gas of $n_{\rm e}=5.3 \times 10^{-3}$ cm$^{-3}$, a thermal pressure $P/k = 3000$ K cm$^{-3}$, an \ion{O}{6} density of $4.2 \times 10^{-7}$ cm$^{-3}$, and a path length through the emitting gas of 250 pc.  The color excess toward NGC~625 is $E($\bv)\ = 0.016, which attenuates emission at 1032 \AA\ by $\sim$ 20\%.  Correcting for this attenuation raises the density and pressure and reduces the path length by the same factor.

\citet{Shelton:07} use shadowing arguments to conclude that essentially all of the \ion{O}{6}\ emission seen along sight line C15301 (at $l = 278.7, b = -47.1$ in \fig{fig_map}) comes from the Galactic halo.  Lacking a measurement of the \ion{O}{6}\ column density along this line of sight, they adopt an average of the published measurements for four nearby sight lines, $\log N$ = 14.37, from which they derive an electron density $n_{\rm e}$ = 1.1--1.6 $\times 10^{-2}$ cm$^{-3}$,  a thermal pressure $P/k = $7--10$ \times 10^3$ K cm$^{-3}$, and a path length of 50--70 pc for the emitting gas.  These parameters are consistent with those derived from the Fairall~9 and NGC~625 data, suggesting a thick disk/halo origin for the \ion{O}{6} -emitting gas along all three lines of sight.

We can derive a lower limit to the distance of the \ion{O}{6} -emitting gas from the angular distance between a pair of \ion{O}{6}\ detection and upper-limit sight lines that are near one another on the sky.  The two closest pairs are I20505/B12901 and C15301/Z90719, but both probe variations in the opacity of an intervening dust cloud (see the discussion in Appendix A2 of \citetalias{Dixon:06}), rather than variations in the intrinsic \ion{O}{6}\ emission.  The third closest pair, C07601/S90522, is separated by $\sim$ 3\arcdeg.  The non-detection of \ion{O}{6}\ along sight line S90522 is not due to interstellar opacity; the extinction maps of \citet{Schlegel:98} suggest that it is less affected by dust than is C07601.  If the \ion{O}{6} -emitting region sampled by sight line C07601 has a radius of $\sim$ 100 pc (assuming size $\sim$ path length), then it lies at least 2 kpc from the Sun and at least 800 pc from the Galactic plane.

\subsection{Comparison with Models} \label{sec_models}

A successful model of the hot component of the interstellar medium must reproduce our observational results:  Diffuse \ion{O}{6}\ emission (i.e., emission unrelated to discrete supernova remnants or superbubbles) is present over the entire sky with intensities between about 2 and 6 kLU.  The emission is patchy: of the sight lines providing statistically-significant results, roughly 40\% yield upper limits $I$(\ion{O}{6})\ $< 2$ kLU.  Near the plane, the emitting regions are less than about 0.15 pc in spatial extent, with electron densities $n_{\rm e} = 0.2-0.3$ cm$^{-3}$  (\citetalias{Dixon:06}).  At high latitudes, the emitting regions are large, with path lengths on the order of 100 pc, and at least 800 kpc from the plane.  Electron densities are on the order of $10^{-2}$ cm$^{-3}$

In a series of papers, \citet{deAvillez:04, deAvillez:05, deAvillezOVI} present the results of high-resolution, three-dimensional hydrodynamic and magnetohydrodynamic simulations of the ISM.  The authors model a section of the Galaxy centered on the solar circle having an area of 1 kpc$^2$ and extending $\pm$ 10 kpc from the Galactic plane.  They employ an adaptive mesh refinement algorithm whose resolution peaks at 1.25 pc within the disk ($|z| \leq 500$ pc).  By computing $N$(\osix)\ along hundreds of sight lines (all with $|z| \leq 250$ pc and $d \leq 1$ kpc) through their data cube, \citet{deAvillezOVI} are able to reproduce both the observed distribution of $N$(\osix)\ with distance and its dispersion.

We derive electron densities $n_{\rm e} \sim 10^{-2}$ cm$^{-3}$ for the \ion{O}{6}-emitting gas along the lines of sight toward Fairall~9 and NGC~625.  \citet[see their Fig.\ 2]{deAvillez:05} present a two-dimensional vertical slice (perpendicular to the midplane) through their three-dimensional data cube showing the density distribution of the ISM.  Gas parcels with densities on the order of $10^{-2}$ cm$^{-3}$ are present throughout the frothy thick disk of ionized and neutral gas lofted by supernova explosions in the plane.  The boundaries of these parcels would be natural locations for the formation of \ion{O}{6} -bearing interfaces.  Model predictions of $N$(\osix)\ and $I$(\ion{O}{6})\ as functions of Galactic latitude have not yet been published.

\subsection{\ion{O}{6}\ Emission from the Magellanic System} \label{sec_magellanic}

The three sight lines in \fig{fig_map} with high-velocity \ion{O}{6}\ emission are S70504 (+84 km s$^{-1}$) and S90513 (+115 km s$^{-1}$) from the current sample and I20505 (+206 km s$^{-1}$) from \citetalias{Dixon:06}.  All three lie in a region of the Magellanic System designated as the ``interface region'' by \citet[see their Fig.\ 4]{Bruns:05}.  The interface region connects the Magellanic Clouds and the Magellanic Bridge with the Magellanic Stream, which lies to the south of $-60\arcdeg$ latitude.  The \ion{H}{1}\ in this region exhibits a complex filamentary structure and a distinct velocity signature.  Sight lines S90513 and I20505 lie near the
projected western and eastern edges of the region, respectively, and the observed
LSR velocities of their \ion{O}{6}\ emission closely match those of the \ion{H}{1}.
Although the \ion{O}{6}\ velocity along sight line S70504 is about half that of the \ion{H}{1}\ in the same direction, it is within the overall range of \ion{H}{1}\ velocities detected in the interface region, 60--360 km s$^{-1}$.

The interface region of the Magellanic System lies about 40 kpc from the Galactic plane \citep{Jin:08} and is thus embedded in the hot ($10^6$ K) Galactic corona.  The perimeters of these high-velocity \ion{H}{1}\ clouds, where cool and hot gas meet and mingle, are natural sites for the formation of intermediate-temperature \ion{O}{6} -bearing gas.  Indeed, \cite{Sembach:03} report \ion{O}{6}\ absorption along several extragalactic sight lines (including Fairall~9) that probe the Magellanic Stream at velocities consistent with that of the \ion{H}{1}\ gas.  Intriguingly, while both Fairall~9 and NGC~625 show \ion{O}{6}\ absorption at Magellanic velocities, neither shows high-velocity \ion{O}{6}\ emission.  The interface region, which does show \ion{O}{6}\ emission, is unique in this respect.

These are the first detections of high-ionization emission from the Magellanic System outside of the Clouds themselves.  The \ion{O}{6}\ intensities observed along the two sight lines towards the edges of the interface region are well within the normal range observed in the diffuse ISM, but the intensity along sight line S70504 (10.5 kLU) is significantly higher.  In fact, it is the highest diffuse \ion{O}{6}\ intensity observed to date (outside of supernova remnants, superbubbles, and high-ionization planetary nebulae).  Though the \ion{O}{6}\ emission feature in this spectrum is statistically significant, its exposure time is quite short, just over 2 ks.  Deeper and more detailed observations would help to determine whether such high intensities are commonly obtained in the interface region of the Magellanic System.

\section{Conclusions}\label{sec_conclusions}

We present the final installment of the {\it FUSE}\/ survey of diffuse \ion{O}{6}\ emission in the interstellar medium.  These observations reveal the large-scale structure of the \ion{O}{6} -bearing gas in the quadrant of the sky centered on the Magellanic Clouds.  Its most prominent feature, a layer of low-velocity \ion{O}{6}\ emission extending more than 70\arcdeg\ from the Galactic plane, is produced by two distinct populations of emitting clouds.  At latitudes $|b| < 30\arcdeg$, sight lines suffer significant extinction, suggesting that they probe relatively nearby emitting regions; their emission features are more likely to be narrow or unresolved, suggesting single interfaces less than about 0.15 pc across; and their velocities are generally consistent with Galactic rotation.  We identify these emitting regions with narrow, high-density interfaces in the local ISM.

At latitudes $|b| > 30\arcdeg$, extinction is low.  Intensities fall with distance from the plane.  Emission features are generally broad, suggesting that they sample turbulent gas or multiple emitting regions spanning a range of velocities.  The \ion{O}{6} -bearing gas seems to be moving away from the Galactic plane.  For two sight lines, Fairall~9 and NGC~625, we combine \ion{O}{6} -emission and -absorption measurements to constrain the physical parameters of the emitting regions.  From the resulting path lengths, we estimate that these regions lie at least 800 pc from the Galactic plane.  The presence of nearby sight lines yielding null detections but strong upper limits suggests that the emission is patchy, consistent with the results of \citet{Howk:02}.

High-velocity \ion{O}{6}\ emission is seen along three sight lines that probe the interface region of the Magellanic System.  The \ion{O}{6}\ velocities are generally consistent with those of the underlying \ion{H}{1}.  High-velocity \ion{O}{6}\ emission is not seen in sight lines that probe the Magellanic Stream, suggesting that the dynamics of the interface region differ from those of the Stream itself.  These are the first detections of emission from high-ionization species in the Magellanic System outside of the Clouds themselves.

\acknowledgments

The authors would like to thank B. P. Wakker for constructing Figure \ref{fig_map}, for providing \ion{O}{6}\ absorption-line data in advance of publication, and for helpful comments on the text.  We acknowledge with gratitude the extraordinary efforts of the {\it FUSE}\/ operations team to make this mission successful.  This research has made use of the NASA Astrophysics Data System (ADS) and the Multimission Archive at the Space Telescope Science Institute (MAST).  STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NAG5-7584 and by other grants and contracts.
The curve-fitting program {\small SPECFIT}\ runs in the IRAF environment.
The Image Reduction and Analysis Facility is distributed by the National Optical Astronomy Observatories, which is supported by the Association of Universities for Research in Astronomy (AURA), Inc., under cooperative agreement with the National Science Foundation.
This work is supported by NASA grant NAS5-32985 to the Johns Hopkins University.

{\it Facilities:} \facility{FUSE}.

redpajama_set_name: RedPajamaArXiv


From the beginning we were met with nothing but the most professional courteousness. People you could trust who cared about your pets, your schedule and your home. I really can't say enough to illustrate what the difference is between Tribeca and the other services we had tried. We use them for everything and are completely happy. We feel fortunate to have a relationship with them.
Whether traveling domestically or internationally by land, air or sea we can customize a travel plan just for you. We are experts in making domestic, foreign and overseas travel arrangements. Our team of caring experts will ensure that your pet travels safely and comfortably door-to-door nationwide or anywhere in the world.


The schefflera houseplant is a popular plant and comes in many varieties. The most well known are the umbrella tree and the dwarf umbrella tree. One of the reasons the plant is popular is because schefflera plant care is so easy, but, while schefflera care is easy, the plant does need to be cared for. Keep reading to learn more about growing schefflera and keeping it healthy and lush.
There are two very important parts to proper schefflera care. The first is correct sunlight and the second is proper watering.
Light – Schefflera plants are medium light plants, which means that they need bright but indirect light. A common complaint about schefflera plants is that they get leggy and floppy. This problem is caused by too little light. Making sure that you are growing schefflera in the right kind of light will help prevent leggy growth. On the other side, you do not want to place a schefflera houseplant in direct, bright light, as this will burn the leaves.
Water – When growing schefflera, be aware that watering correctly will help to keep your schefflera houseplant healthy. To water correctly, wait until the soil in the pot dries out and then thoroughly soak the soil when you water. Often, people will over water their schefflera plant and this will eventually kill it. Yellow leaves that fall off the plant is a sign that you may be watering too much.
Additional care of schefflera includes pruning and fertilization.
Pruning – Your schefflera may also need to be pruned occasionally, especially if it is not getting quite enough light. Pruning a schefflera is simple. Just cut off what you feel is overgrown or leggy back to a size or shape you like. Schefflera houseplants rebound quickly from pruning and will look even fuller and more lush shortly after pruning.
Fertilizer – You do not need to fertilize your schefflera, but if you would like to, you can give it a half solution water soluble fertilizer once a year.
Schefflera plants are poisonous to people and animals, if eaten. It is not often fatal but will cause a burning sensation, swelling, difficulty swallowing, and in severe cases, difficult breathing.
Schefflera plants are not often bothered by pests or disease, but it can happen occasionally.
Spider mites and mealybugs are the most common pests that affect schefflera plants. In light cases of infestation, washing the plant with water and soap will normally eliminate the pests. With heavier infestations, you many need to treat the plant with an insecticide like neem oil. Also, be aware that pests typically attack this plant if it is stressed. If your schefflera has pests, this is likely a sign it is either getting too little light or too much water.
The most common disease that affects schefflera is root rot. This disease is brought on by overwatering and poor drainage in the soil.


Delicate artichoke hearts are processed into a true delicacy with the finest vegetables and olive oil. This family recipe will have you coming back for more. Serve this Sicilian caponata as an antipasto or with grilled meat or fish. It is also enjoyed on slices of crusty bread or add as a spread to your sandwiches.
Ingredients: Artichoke 70%, green olives 8%, tomato 8%, pine nuts, celery, capers, onions, carrots, olive oil, salt, sugar, wine vinegar, flavoring. Antioxidants: citric acid, ascorbic acid.


"Starship Troopers" RiffTrax brings back Mystery Science Theater Laughs!
I have so many great memories in my life; many stemming from cheesy monster movies. As a kid I was glued to the television set every Saturday afternoon for the CREATURE DOUBLE FEATURE and as an adult, I was glued to the television set every Saturday night for MYSTERY SCIENCE THEATER 3000! It was such a disappointment when Comedy Central cancelled MST3K and the SyFy Channel picked it up. Like all good things, the SyFy Channel usually ruins it. Thankfully it wasn't long before the guys who made a career out of riffing on movies, something many of us did anyway, went on to create CINEMA TITANIC, THE FILM CREW and RIFFTRAX, all variations of the original concept.
As of this writing, to my knowledge, RIFFTRAX is the only remaining of the three projects and it stars MST3K alums Michael J. Nelson, Kevin Murphy and Bill Corbett. They pretty much do the same thing that either Joel or Mike did with Crow T. Robot and Tom Servo, but only now they do it live on stage in front of a packed audience of MST3K fans.
I have seen many of their DVD releases and at times, their live show is broadcast nationally at local movie theaters, usually showing the public domain films we are all accustomed to. Just recently, however, RIFFTRAX presented somewhat of a blockbuster film (by their standards) to be riffed on, STARSHIP TROOPERS, from 1997. This was with the help of a kick-starter program and this presentation (shown LIVE a month ago) was an encore.
STARSHIP TROOPERS got mixed reviews at the time of its release but to me it was a fun and exciting movie. It featured a great cast including Casper Van Dien, Denise Richards, Dina Meyer, Neil Patrick Harris and Jake Busey (many of whom supported the kick-starter program). The story was also very well put together with amazing special effects, including some of the best CGI effects ever put to film. When it was announced that this great sci-fi films was going to be the target of riffing, I had no idea what to expect. Thankfully, Mike, Kevin and Bill did not disappoint. They took an already great film and made it even greater!
The jokes throughout were fast and furious and there were many nods to the MST3K days, that only devout fans would get. No one was spared their wrath, especially Denise Richard, who set up their jokes thanks to the blank stare she always seems to have going on.
I truly love seeing these presentations because they are always a guaranteed good time and the people who are in the audience with you are people who actually get it. To this day I still have people who say they hated MST3K because when they watch a movie, they don't want people talking through it. They clearly didn't get it. It makes for a much greater viewing experience when you are surrounded by people who are laughing at the very same thing you are laughing at and who truly appreciate what these three comic geniuses are all about. If RIFFTRAX ever comes to a city near you, make sure you check it out! You will be glad you did (and you will probably find yourself pulling out those circulated tapes of yesteryear to relive the magic that was MYSTERY SCIENCE THEATER 3000)!
This entry was posted in Horror Hosts, Science Fiction and tagged Bill Corbett, Casper Van Dien, Creature Double Feature, Crow T. Robot, Denise Richards, Dina Meyer, Jake Busey, Kevin Murphy, Michael J. Nelson, MST3K, Mystery Science Theater 3000, Neil Patrick Harris, Rifftrax, Starship Troopers, SyFy Channel, Tom Servo. Bookmark the permalink.
← Delving into the Dynamics of Svengoolie's New Coffin!
My husband and I were at the August showing and had a blast! It was hilarious. We can't wait for Rifftrax Live: Night of the Living Dead next month on the 24th.


Q: How far in advanced should we book?
bookings in the same calendar year.
Of course. However, I do not share those files with my clients.
Q: How did you end up in photography?
photography have always been a part of my life.
Q: I'm pregnant, when should I do my maternity shoots?
Seven to eight months is a perfect window.
Q: When do you recommend I schedule a newborn shoot?
four weeks after your due date.
Q: Will you travel to my home for my newborn shoot?
Absolutely! Sit back and relax with your new babe. I'll take care of the rest.
For portrait photography 4-6 weeks, if not otherwise discussed.
For wedding photography 3-4 months, if not otherwise discussed.
able to share, download, and order prints right from the gallery.
Q: What should I wear for portrait sessions?
Q: So you're a designer too?
Yup yup, I split my time almost evenly between design and photography.
Check out my link here.
Q: What's your beverage of choice?
adult beverages, then I'm going with Matilda beer or any red wine.


This morning I was oil pulling on Snapchat (username: organic_olivia) and got a ton of questions about the benefits of this practice. I also had a lovely snap friend send me a message saying that oil pulling cleared up her skin, which is partly due its detoxification benefits! There are a ton of lymph nodes on or around the jaw that get pumped as you swish the oil in your mouth. I already have a blog post about this (click here to read) but wanted to post a refresher!
"As simple as it is, oil pulling has a very powerful detoxifying effect. Our mouths are the home to billions of bacteria, viruses, and fungi. Candida and Streptococcus are common residents in our mouths. It's these types of germs and their toxic waste products that cause gum disease and tooth decay and contribute to many other health problems including arthritis and heart disease. Our immune system is constantly fighting these troublemakers. If our immune system becomes overloaded or burdened by excessive stress, poor diet, environmental toxins and such, these organisms can spread throughout the body causing secondary infections and chronic inflammation, leading to any number of health problems." – Bruce Fife, ND.
This is so important because illness begins in the mouth and the gut!
Oil pulling is an ancient Ayurvedic dental technique. In a study from 2008 including 20 adolescents, oil pulling caused a reduction in the number of Streptococcus Mutans in plaque in as little as 2 weeks. The benefits of oil pulling (especially with anti-bacterial, anti-fungal coconut oil) reduce the inflammatory pathogenic burden not only in the mouth, but in the whole body – which means you'll have more energy, since your body isn't focusing on fighting that load. You will notice whiter teeth, better breath, healthier gums, increased energy/metabolism, & less sensitive teeth.
SIDE NOTE – I couldn't oil pull at first because I'm SO squeamish when it comes to certain tastes and textures! What I do to make it palatable is: I make sure it's in liquid form, then I mix in 1 tsp. birch xylitol (a sweetener made from trees that tastes like sugar but actually kills bacteria & destroys biofilms!) I also add lemon essential oil. As I swish, the xylitol crystals dissolve into the oil and it tastes like lemon candy.


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Are you ready for Brexit?
by Dr. Eleanor Grimes On October 23rd two regulatory specialists from UL attended the Brexit Chemicals Stakeholder Event held by DEFRA and the HSE. The...
Commission Implementing Regulation Clarifies Rules for Phase-in Substances under REACH
by Dr. Martina Schneider On October 10, 2019, the European Commission clarified which provisions for phase-in substances will apply after December 31, 2019. Under Regulation...
UL Launches LOLI® Illuminator!
We are delighted to announce the immediate availability of LOLI® Illuminator, a first-of-its-kind software tool enabling self-service access to high-quality chemical regulatory data monitoring. You...
Top Searched Plastics and Chemicals Terms on UL's Prospector®
Understanding what chemical and plastics buyers are searching for is key to creating a solid marketing strategy. Having this knowledge allows you to align your...
IUCLID Software to be Updated to Allow Submission of Additional Information on Nanomaterials under REACH
by Dr. Martina Schneider and Caroline Miller, CIH, CSP On December 3, 2018, the EU amended the REACH Regulation via Commission Regulation (EU) 2018/1881 to...
3 Ways Prospector® Helps You Win at Search Engine Marketing
Why do you need Prospector? Chemical marketing has changed a lot over the last 5 years According to Adobe, 76% of marketers think that marketing...
Test Methods Updated Measuring Toxicological and Ecotoxicological Properties of Chemicals for REACH
by Dr. Martina Schneider In order to keep up with technical progress and reduce the need for animal testing, the EU has been adopting the...
European Commission adopts the 14th ATP to CLP which includes harmonised classification and labeling for titanium dioxide
by Charlotte Blackburn, PhD The 14th ATP (Adaptation to Technical Progress) to the CLP regulation, which includes amendments to Annexes II, III and VI, has...
Changes and Amendments to the IATA Dangerous Goods Regulations (DGR) 61st edition 2020
by Tatjana Benko and John Stewart PhD This article highlights some of the important changes and amendments introduced to the 61st edition of the IATA...
Brazil Updates ABNT Classification (NBR 14725) Standard
by Caroline Miller, CIH, CSP In June, the Brazil Association of Technical Standards (ABNT) updated its standards for classifying chemicals, bringing it in line with...
Come & See UL at in-cosmetics Asia!
November 5 - 7, 2019
Download Cora Knutson's Cosmetics Presentation from In-Cosmetics Latin America, São Paulo
UL Senior Regulatory Specialist Cora Knutson recently spoke at the In-Cosmetics Latin America exhibition in São Paulo, Brazil, where she presented a technical seminar titled...
Poison Centres: The First CLP Annex VIII Compliance Date for Mixtures for Consumer Use Agreed to be Postponed
By Dr. Charlotte Blackburn, Regulatory Specialist At the 31st meeting of the Competent Authorities for REACH and CLP (CARACAL), held on 18th September 2019, the...
EPA Posts Update to TSCA Inventory
by John J. Kowalski, CHMM On September 19, 2019, the U.S. Environmental Protection Agency (EPA or the Agency) posted an update to the public version of...
Poison Centres: A Guide for Annex VIII Compliance [checklist]
Do you need to submit a Poison Centre Notification? In an attempt to harmonise Poison Centre information across the EU, Annex VIII to CLP was...
New Draft Version of REACH Annex II on the Format of the SDS Released
by Dr. Eleanor Grimes Annex II of REACH, which sets out the required structure and content for a safety data sheet (SDS), has had a...
ECHA Publishes Information Requirements for SCIP Database
by Ancuta Rusu, PhD Pushing towards a Circular Economy where the generation of waste is minimized, in particular waste containing hazardous substances, ECHA has set...
U.S. – New York State, Disclosure of Chemicals in Household Cleansers Requirements Invalid
by Caroline Miller, CIH, CSP The New York State Department of Environmental Conservation (NYSDEC) Household Cleansing Product Information Disclosure Program has been overturned by the...
UL's Karen Lintz to Speak at in-cosmetics North America
Come & See UL at in-cosmetics North America!
If you're in New York from October 23-24, be sure to visit the UL booth at in-cosmetics North America!
UL's Cora Knutson To Speak At In-Cosmetics Latin America
Come & See UL at in-cosmetics Latin America!
If you're in São Paulo, Brazil from September 18-19, be sure to visit the UL booth at in-cosmetics Latin America!
Western Australia's Proposed New Work Health and Safety Regulations
by Laura Whiteman Western Australia's health and safety laws are in the process of being modernised. This is part of harmonising the legislation and codes...
TSCA: What You Need To Know About New Chemical Notification Obligations – Myth or Fact Part 3
By Ghassan Zughaib, Senior Regulatory Specialist The U.S. Congress originally enacted the Toxic Substances Control Act (TSCA) in 1976 and significantly amended it in 2016. However,...
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redpajama_set_name: RedPajamaCommonCrawl


Most individuals obtain International Journal of Cultic Studies (IJCS) as one of their membership benefits in the International Cultic Studies Association (ICSA). Membership Info.
Nonmembers – $45/yr. (USA); $65/yr. (outside USA).
To subscribe, send a check (US dollars drawn on a US bank) or Visa or MasterCard information to ICSA, PO Box 2265, Bonita Springs, FL 34133 (mail@icsamail.com; 1-239-514-3081). Or, subscribe online.


As you can see I am trying to use Oracle12c's identity columns.
However Hibernate doesn't seem to be able to retrieve the generated id. I guess that the ROWID of the inserted tuple is being retrieved instead of the actual id, therefore a conversion error is raised and the whole transaction is aborted.


text:
HomeAnalysisYahoo News story accidentally admits most children..[outbreak] vaccinated against measles
Yahoo News story accidentally admits most children..[outbreak] vaccinated against measles
February 5, 2019 This article was posted by TLB Staff Analysis, HEALTH, MEDIA, Spotlight 0
Yahoo News story accidentally admits most children infected with measles outbreak were already vaccinated against measles
By Ethan Huff
In announcing a trumped up "state of emergency" that was recently declared by Washington Governor Jay Inslee in response to a measles outbreak in Clark County, Yahoo News accidentally let it slip that most of the children affected had actually been previously vaccinated against the disease – once again proving that vaccines don't work.
Contrary to the mainstream media's unsubstantiated narrative that this latest measles outbreak, like many others in the past, was supposedly caused by "the anti-vaccine movement," it's now apparent that it was actually a total failure of the MMR vaccine for measles, mumps, and rubella that resulted in children getting sick.
"The majority of those infected are children, many of whom have not been immunized against the disease," reported AFP News, and republished by Yahoo News, indicating that at least some of the children stricken with measles had received the MMR in accordance with CDC (Centers for Disease Control and Prevention) guidelines.
Why we're surmising that it was actually most of the kids, however, has to do with the article's tricky wording. Had most of the children who've contracted measles not previously been vaccinated with MMR as insinuated, you can be sure that Yahoo and AFP would have clearly indicated this.
"The majority of those infected are children, most of whom have not been immunized against the disease," would have been the quote. But instead of using the word "most," the article instead uses the word "many" – which, if you read between the lines, suggests that at least half of the affected children were previously vaccinated with MMR.
Big Vaccine constantly manufacturers disease outbreak crises like this to scare parents into vaccinating
The same news report goes on to quote Governor Jay Inslee, who gave an absurd public statement claiming that measles "is a highly contagious infectious disease that can be fatal in small children" – the suggestion being that parents had better vaccinate their children if they don't want them to die.
But, as usual, this is just another trumped up falsehood, seeing as how measles was viewed in the past as being no more severe than common chickenpox. In fact, an old episode of "The Brady Bunch" referred to measles as the "best" disease for a child to get if he or she has to be sick with something.
[Video insert by TLB]
The great thing about naturally contracting measles is that, once you recover, you're immune from the disease for life. The same can't be said for the MMR vaccine, however, which only provides temporary protection at best.
For Governor Inslee and the mainstream media to convey a message of death in conjunction with measles, along with a declaration of a state of emergency, is just more mindless fear-mongering at the behest of Big Vaccine, which is losing considerable market share as more and more parents refuse vaccines for their children.
It has nothing to do with safety, and everything to do with vaccine industry profits, which suffer whenever parents make the decision to allow their children to develop immunity naturally instead of injecting them with aborted human fetal tissue, cancer-causing chemicals, and other harmful vaccine additives.
Even right-leaning news outlets like The Daily Caller are guilty of spreading vaccine industry lies that try to scare parents into getting their children jabbed, which puts these little ones at risk of serious complications and even death.
The truth of the matter is that a mere 26 children came down with the measles in this latest outbreak, and most of them were already vaccinated. If the MMR vaccine really worked, and Governor Inslee's comments were valid, this number would be zero, and all of the children affected would be dead – which none of them are.
(TLB) published this article from Vaccine Jihad with our appreciation for the coverage.
Other Articles by Ethan Huff
The Liberty Beacon Project is now expanding at a near exponential rate, and for this we are grateful and excited! But we must also be practical. For 7 years we have not asked for any donations, and have built this project with our own funds as we grew. We are now experiencing ever increasing growing pains due to the large number of websites and projects we represent. So we have just installed donation buttons on our websites and ask that you consider this when you visit them. Nothing is too small. We thank you for all your support and your considerations … (TLB)
Disclaimer: The Liberty Beacon contains copyrighted material the use of which has not always been specifically authorized by the copyright owner. We are making such material available to our readers under the provisions of "fair use" in an effort to advance a better understanding of political, health, economic and social issues. The material on this site is distributed without profit to those who have expressed a prior interest in receiving it for research and educational purposes. If you wish to use copyrighted material for purposes other than "fair use" you must request permission from the copyright owner.
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natural immunity
Vaccine Propaganda
Columbus Day Proves History is.. Celebrating Mass Murder
EBOLA, DRUG-RESISTANT TB, DENGUE FEVER ARE COMING INTO THE U.S.
Vaccine Court Awards Millions to Two Children With Autism


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Cygnus Spacecraft Departs International Space Station
Northrop Grumman Corporation announced on Friday that its Cygnus spacecraft has departed from the International Space Station after an 81-day stay during the NG-10 mission.
While docked, astronauts unloaded approximately 7,400 pounds of vital supplies and scientific equipment. The Slingshot CubeSat Deployer System, a new commercial customer for Cygnus, was also installed for its inaugural flight on the spacecraft. Slingshot, a flexible platform that can fly hosted payloads and CubeSats, further demonstrates the ability of Cygnus to host multiple secondary payloads as part of a single mission. Cygnus departed from the International Space Station at 11:16 a.m. EST loaded with more than 2,500 kilograms (5,500 pounds) of disposal cargo.
The S.S. John Young now begins the second half of its mission by repositioning above the station to deploy two CubeSats via the NanoRacks External Cygnus Deployer and two CubeSats from the Slingshot CubeSat Deployer. Cygnus will then lower its orbit below the station for another NanoRacks deployment of one CubeSat. This specific satellite deployment operation marks the first dual altitude deployment for Cygnus, further demonstrating the spacecraft's capabilities beyond cargo delivery and removal. During its secondary mission, the spacecraft will also operate a commercial powered payload mounted in the Slingshot launch system as another new customer, UbiquitiLink, Inc. UbiqutiLink's telecommunications payload antenna will test the ability to send and receive messages in areas without ground-based connectivity.
"NG-10 continues to highlight Northrop Grumman's ability to meet the needs of multiple customers throughout one mission to the International Space Station," said Frank DeMauro, vice president and general manager, space systems, Northrop Grumman. "During each trip to the station, Cygnus continues to demonstrate additional capabilities as we partner with new commercial customers. These new relationships will create opportunities for the International Space Station to expand its role as a unique platform for ground-breaking science."
The two NanoRacks CubeSats to be deployed above the station are the Cost-effective High E-Frequency Satellite (CHEFSat) and MYSat-1. CHEFSat tests and prepares consumer communications technology for use in space. MYSat-1 marks the first satellite developed by Khalifa University in Abu Dhabi, United Arab Emirates (UAE). MYSat-1 was developed as part of Khalifa's Space Systems and Technology Concentration, a joint program established in 2015 in collaboration with UAE-based satellite operator Al Yah Satellite Communications Company (Yahsat) and Northrop Grumman. Engineers from both companies helped develop the initial curriculum for the concentration, and provided guidance and mentorship during the design and build phases of the MYSat-1 satellite.
Once the S.S. John Young moves below the International Space Station, KickSat-2, a collaborative CubeSat from NASA Ames Research Center and Stanford University, will be deployed via the NanoRacks Deployer.
The next Cygnus launch, known as the NG-11 mission, will be Northrop Grumman's final launch under the CRS-1 contract and is currently scheduled for spring. During this mission, Cygnus will demonstrate its unique capability to fly solo through space for an extended duration after departing from the station. This innovation is another example of Cygnus's potential to double as a free-flying laboratory for science experiments, technology demonstrations and as a CubeSat launch platform. These enhancements will build on the positive impact of the International Space Station to develop a new economy in low Earth orbit.
The NG-10 mission began Nov. 17, 2018, when Cygnus launched aboard a Northrop Grumman Antares rocket from NASA Wallops Flight Facility in Virginia. The mission is expected to end on Feb. 25, at approximately 3:30 a.m. EST when Cygnus will execute a safe, destructive reentry into the Earth's atmosphere over the Pacific Ocean.
Credit: northropgrumman.com
Tags: astronaut, CubeSat, Cygnus, expedition, ISS, NanoRacks, NASA, Northrop Grumman, space station, spacecraft
You can easily pay your metro pcs payment via online, over the phone, through the mail, or at select authorized payment centers. In this article, we have updated you with the complete information regarding the Metro PCS Bill Pay Login and the various methods to pay your bill.
njmcdirect


text:
Q: How do I find out if a file is a photo or a video in Qt? How do I find out if a file is a photo or a video in Qt?

A: You ask if Qt can tell if something is "a photo or a video", which is ambiguous, but I'll translate it to:
If I have a filename, does Qt have a feature to tell me if that is (a) an image file, (b) a video file, or (c) some other kind of file?
Knowing a file's type can come from a few sources.  There's the extension in the file's name, there's "sniffing" the contents of the file's data and looking for recognized magic header sequences, and there's random metadata which may live somewhere else that's very specific to the applications or OS managing the file.
Someone asked a question which was how to get the "MIME type" of a file in Qt:
Find out the mime type and associated applications with Qt
If you could do that, you could see if the string you got back was in the image/ hierarchy:
http://en.wikipedia.org/wiki/Internet_media_type#Type_image
But there's no Qt functions for that.  So you're left pretty much checking the file extension, or if you specifically want to know if a given file is an image format that Qt can read, then you can use QImageReader::imageFormat() to "sniff" a file:
QByteArray imageFormat = QImageReader::imageFormat(fileName);

If the image is in the set of image types that Qt considers loadable, it will hand back a string of bytes that corresponds to that format.  Otherwise you'll get an empty string.  That isn't to say that failing this test means something isn't an image of some other kind, of course.
As for determining if something is a video file that Qt can play, there seems to be a possibility to do a similar "sniff" of video files if you're using Phonon via MediaSource::type() and checking to see that it's not Phonon::MediaSource::Invalid.

redpajama_set_name: RedPajamaStackExchange


Mullen Group senior VP Richard J. Maloney talks about the new partnership, industry consolidation and the driver shortage.
Jay's Moving and Storage Ltd.
OKOTOKS, Alta. — Even though the majority of its business is in oilfield services, Mullen Group Ltd. is more optimistic about the short-term future of its trucking and logistics operations.
"We're probably a little more bullish on the trucking and logistics part of our business to the extent that it's not going to be huge growth but it's gong to be active," said Richard J. Maloney, Mullen's senior vice-president, adding that he expects the trucking and logistics sector to demonstrate growth of 2% in the coming year.
"I know 2% GDP growth doesn't sound like much, but if it is 2% year-over-year-over-year, there is going to be that inflection point when all the capacity in that market is starting to be taken up by a trucking and logistics perspective.
Oilfield services, we believe there is a little too much capacity right there right now. We're just watching. We may be sitting on the fence a little more for those opportunities. It's not to say they're going to go away. We're a very patient company. We've been around since 1949. The patriarch still walks through here every once in a while. We can wait to see what other opportunities come over the next period of time. We think risk is being mis-priced in terms of what some people are looking for for their organizations, and others can go and have at it. We don't necessarily think it's going to be a long-term phenomena, but we're just cautious.
For Maloney, "this" refers to a Letter of Intent between Mullen and Kriska Holdings Ltd. to enter into partnership. The deal will see Mullen become a 30% partner in the new holding company Kriska Transportation Group. Mullen will also transfer control of Ontario-based LTL carrier Mill Creek to the new entity.
According to Maloney, working more closely with Kriska in the Ontario market makes so much sense that Mullen wanted to make the deal happen any way it could.
"They didn't want to sell," said Maloney.
Since the new arrangement has not been finalized yet—that's expected to happen on October 31—Maloney can't say exactly what Kriska's plans will be, but he did explain that the new company is being built with a single goal in mind.
Maloney believes that many of those consolidation opportunities will come from retiring owners looking to sell their businesses.
"The demographic is consistent throughout North America of the owner/entrepreneurs who are turning 55-65 and now what do they do for an exit strategy? Maybe they are well run companies—at least some of them if not all of them—and those ones are the ones that are looking for an opportunity to maintain their legacy.
As for Mullen's own trucking operations, it will continue to focus on the Western Canadian LTL business, a business it has grown with the acquisitions of Hi-Way 9 Group of Companies, which covers Edmonton and parts to the south, Jay's Moving and Storage Ltd. which reaches across all of Saskatchewan and Grimshaw Trucking LP which travels north from Edmonton.
Overall, Mullen Group has a $100 million capital budget, and approximately 25% of that is spent on its trucking and logistics divisions, including buying new trailers and tractors.
"Trucking and logistics is not as capital intensive as the oilfield services business is, if you have the trailers and you can attract the drivers, which our business units out here do fairly well, we think we have a reasonable chance to succeed," said Maloney.
While Maloney believes Mullen does a good job of attracting drivers, he said the driver shortage is a reality every carrier must face. It's just a case of demographics and math. That's one of the reasons the company some transload and rail-related businesses, including Kleysen Group LP. Moving more freight by rail eases some of the demands on trucks, and leaves the drivers to fill seats in last-mile deliveries.
As for attracting drivers and dock workers to the company Maloney said Mullen not only pays attention to the obvious things like wages, but to other avenues as well.


text:
Hybrid Electric Vehicles, 2nd Edition by Chris Mi, M. Abul Masrur
Get full access to Hybrid Electric Vehicles, 2nd Edition and 60K+ other titles, with free 10-day trial of O'Reilly.
16Wireless Power Transfer for Electric Vehicle Applications
Wireless power transfer (WPT) is the technology which could set people free from annoying wires. In fact, WPT adopts a basic theory that has been developed for at least 30 years under the term inductive power transfer (IPT). WPT technology has been developed rapidly in recent years. At kilowatts power level, the transfer distance increases from several millimeters to several hundred millimeters with a grid to load efficiency above 90%. These advances make WPT very attractive for use in electric vehicle (EV) charging applications in both stationary and dynamic charging scenarios. This chapter reviews the technologies in the WPT area applicable to EV wireless charging. By introducing WPT in EVs, the obstacles of charging time, range and cost can be easily mitigated. Furthermore, battery technology is no longer relevant in the mass market penetration of EVs. It is hoped that researchers, encouraged by state‐of‐the‐art achievements, will continue to push forward and further the development of WPT, as well as the expansion of EVs.
The Sections 16.1–7 introduce the basics of WPT with a focus on the IPT technology, while Section 16.8 discusses a double‐sided LCC topology. Finally, capacitive wireless power transfer is introduced and discussed briefly in Section 16.9.
16.1 Introduction1
Owing to energy, environmental, and many other concerns, the electrification of transportation has been carried out for many years. In railway ...
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One Texas-based company has built a thriving business by turning empty old barns into modern dwellings for today's homeowner.
As agriculture has morphed into big business and populations have shifted from the countryside to urban centers, timber-frame barns have become rare. Thanks to companies like Heritage Restorations, however, many historic barns are being repurposed in exciting ways that their original builders could not have foreseen.
Based in Texas, Heritage Restorations has spent the last 20 years acquiring, carefully dismantling, skillfully rebuilding, and creatively integrating centuries-old barns into stunning new buildings—commercial spaces, event centers, and yes, even private homes. Combined with the best of today's energy efficient materials, timber barn frames have made for jaw-dropping superstructures in residences across the country. It seems that whereas historic barns no longer fit the bill for 21st-century farmers, they provide much of what contemporary homeowners want—ample square footage, open floor plans, and timeless, authentic style.
As alluring as the barns may be in their patinated, hand-hewn beauty, their histories are even more engrossing. Many of these barns survived the Civil War; some are considerably older, dating back to the Colonial era. In fact, in the process of dismantling one barn, Heritage Restorations uncovered a Revolutionary War bayonet hidden behind a wall. Whereas barn-style homes are by no means unprecedented, Heritage Restorations takes a unique approach. Aware of these barns as outstanding examples of early American craftsmanship—and, indeed, as history embodied—the company seeks to preserve as much as possible of the original.
When it began business, members of the company would drive along the backroads of upstate New York and rural New Jersey on the hunt for disused barns. When they found one, they would simply go knock on the door of the adjacent house. In time, and with improved technology, Heritage Restorations adopted more sophisticated methods. The team now uses Google Earth to explore rural areas, narrowing their eyes in search of certain telltale rooflines. But even with satellite imagery available, the company has not outgrown, and perhaps never will, advertisements that list their phone number under a simple message: "We Buy Barns".
Some customers buy only the timber frame, opting to work with their own trusted architect and/or contractor. In that case, Heritage Restorations, besides fumigating the wooden members, provides third-party advice gleaned from the many dozens of barn homes the company has helped to realize in the past. Since working around a reclaimed wood frame presents some challenges, and differs substantially from conventional modern framing, there are bound to be questions.
Other customers retain Heritage Restorations for its in-house architectural services. The company has overseen projects large and small, deploying at least a few different design strategies. One option is for the home to be fully contained within the original barn frame. For additional square footage, multiple frames may be combined into a single building. And in still another permutation, the barn frame may be supplemented by one or more conventionally framed additions. Though specifics change, of course, from site to site and project to project, there's one commonality in all: hundreds of years after its raising, the barn still stands.
For more information, visit Heritage Restorations.


Avoid food boredom in the dorms with these meal ideas if you have a microwave, mini refrigerator, shared kitchen or no appliances.
Bread, vegetables, fruit, yogurt and deli meats are all options for mini refrigerators.
The first few weeks of college are exciting –– new friends, lifestyle and food. At first, it seems like the cafeteria options might never get old. After all, who could grow tired of a salad bar, MYO wrap station and ice cream bar? But after a bit of time, the average college student will tell you that the food in the dining hall always wears out its welcome.
Luckily, there's an app for that. Well, not exactly. There is, however, a solution and it comes in the form of a few simple food items that can be kept on hand whether you have a microwave, mini fridge, shared kitchen area on your floor or no appliances at all. Check out these solutions for do-it-yourself meal preparation and say goodbye to cafeteria food boredom.
Sure, a microwave allows for frozen meals and experts say healthier choices, like Lean Cuisine, are a better choice when options are limited. Keep in mind, however, that these frozen dinners are typically loaded with sodium and should not be a regular choice. Stacey Burke, a nutrition educator and coach, said a microwave can also be used for quick, healthy meal ideas and additions, like vegetables.
"Vegetables can easily be steamed in the microwave," she said. "Just add a little water to a heat-safe dish and steam anything from broccoli or cauliflower to kale or spinach. Rice, couscous and quinoa are all healthy grains that can also be prepared simply by heating water to a boil in the microwave, and adding the grain to soak for 5 to ten minutes. Combine your steamed veggies and whole grains for a healthy microwave 'stir-fry'."
"Spray a bowl with cooking oil spray, stir egg or use a liquid egg substitute, and heat for 30 seconds," she said. "Check on it, stir and cook in 30 second increments until cooked. Eat with fresh vegetables, fruit or on a sandwich."
A small refrigerator can be a lifesaver when it comes to beating food boredom. Sophie Skover, who is known as "The Food Craving Coach" and author of "The Continuous Appetite," said whole grain bread, low-fat cheese, low-sodium deli meats and spinach are all food items that are easy to keep on hand for a quick sandwich.
Hugh said milk, soy milk, greek yogurt, baby carrots, cut celery and hummus are also ideal food options for a mini refrigerator.
Stock the kitchen with a cheap strainer and can opener that can be kept in your room or stored in a cabinet for the whole floor to share. Buy canned beans and vegetables, and a variety of spices that you can keep in your dorm closet and tote down to kitchen when you are ready for a fresh meal. Diane and Tom Griesel, co-authors of "TurboCharged" and "TurboCharged Recipes" said these healthy canned solutions make for an filling meal that can easily be prepared in a shared kitchen space.
Skover said reusable containers can also come in handy when using a shared kitchen space. Prepare chicken, eggs, rice, pasta or a salad within the space, and then store in containers for on-the-go options.
Skover emphasizes that while the lack of available appliances might lead a student to more dining hall experiences, there are tricks for ensuring that a meal is healthy and satisfying.
"Use your meal plan and see your part broken into three parts: one for protein, one for veggies and one for a whole grain carbohydrate," she said. "Try to stick to that."
Fruit, water, raw nuts, protein bars and powders, vacuum packs of tuna or salmon, whole grain crackers, and almond or peanut butter are all healthy food options that can easily be stores in a dorm room closet with no refrigeration or tools for preparation required.
And always keep in mind, said Skover: "You can be healthy anywhere you go. All it takes is a little pre-thought, intention and follow through!"
Steam veggies and store-bought boxes of rice or pasta in the microwave for an easy meal.
Take advantage of kitchen tools, like a strainer or can opener, for use in a shared kitchen space.
Raw nuts, protein bars, fruit and instant oatmeal are all food choices that can be stored in a dorm room.


text:
What Brought about the Modern City?
What Brought about the Modern City?What Brought about the Modern City?
The modern city was brought about by the process of industrialization. During industrialization, there was vast growth of manufacturing, marketing, labor, management, systems of communication and transportation, and growth of finance which brought about the industrial city. This indicates that the modern city was a product of the industrialization process. During this period of time, the existing cities acted as magnets whereby many people were pulled from the American countryside and from foreign countries. What Brought about the Modern City? As people converged into one central position, and started conducting their businesses, these small cities became big cities as they were occupied by many people from different regions.
On the other hand, life changed as people increased migrating to urban areas. The apartments present could not handle all the people hence resulting in overcrowding and creation of slums. There was stiff competition for the existing social amenities like water and electricity. Only the middle class people managed staying within the city while the poor resided in slums. Increase in industries resulted in environmental pollution which when combined with overcrowding resulted to increased diseases like cholera and typhoid. The poor could not afford medical care hence there was an increase in death rates.What Brought about the Modern City?
Religion in the Middle East
Uses of Cell Phones


"A Risk Questionnaire was designed by INCEF in partnership with local community members and with technical input provided by US Centers for Disease Control and Prevention. The questionnaire was created to capture and better understand presumptive risk factors for MPXV infection and the population that is most likely to participate in these activities, with the objective of improving the specificity and efficacy of outreach materials for populations in rural DRC. This survey was performed in Tshuapa Province, DRC, a rural, forested area of the Congo Basin, in which MPX is endemic. To our knowledge, this questionnaire is the first of its kind, to be conducted in this population by the investigators."
European Commission, Directorate-General for International Cooperation and Development. (2015). Larger than elephants: Inputs for an EU strategic approach to wildlife conservation in Africa – Synthesis.
Collins, Julia. (2017). Filmmaker Cynthia Moses effects change in Congolese Communities [Blog post]. Girls Like You and Me.
"Filmmaker Cynthia Moses grew up in Central Massachusetts, where she thought life would bring a husband, kids, and a white picket fence. Then, she joined the Peace Corps in the early 1970s and left that life behind. After stints at ABC and 60 Minutes, Cynthia took a job with National Geographic's wildlife documentary unit, and became fascinated with chimpanzees, gorillas. Several years filming in their native habitats in Central Africa led Cynthia to start INCEF, which makes films by and for local people to communicate ideas at the intersections of education, public health, and conservation. Cynthia and her team have reached over a million people over the past ten years, and today, Cynthia is focused on creating foundations for INCEF's work to continue long into the future."


2.	Promotion commences at 12:00am AEST on 22 September 2018 and closes on 28 September 2019 at 11.59 pm AEST (Promotion Period).
(5) click on "Enter Promotion".
9.	Multiple Entries permitted, subject to the following: (a) a maximum of one (1) Entry may be submitted per Huggies® Club Member per week (i.e. Wednesday to Tuesday); and (b) each Entry must be submitted separately and in accordance with the Conditions of Entry.
12.	There will be four (4) draws conducted for this Promotion (each a Draw). Entries into each Draw will open at 12:00am and close at 11:59pm on the dates outlined in the table below. Each Draw will be held at Level 2, 85 Commonwealth Street Surry Hills NSW 2010 Australia at 2:00pm on the dates outlined in the table below. Entries in each Draw will NOT be entered into any subsequent Draw(s). All times indicated are in AEST/AEDST as per local NSW time. Winners will be notified in writing by email within two (2) business days of the relevant Draw, and each winner's name will also be published on the Promotion Website on the dates outlined in the table below.
e) 6 packs of Huggies® Little Swimmers Swim Pants (in size and variety requested by the winner), valued at up to $89.95.
14.	The total Prize pool value is up to a maximum of $2,560.00. The value of the Prize is accurate at the date of commencement of the Promotion Period and based upon the recommended retail prices at the date of printing. The Promoter accepts no responsibility for any variation in the value of the Prize after that date.
17.	The Promoter may conduct such further draws as are necessary for any unclaimed Prize at the same time and place as the original Draws at 4:00pm AEST/AEDST on the dates outlined in the table below, subject however to any directions given by any applicable gaming authorities. The winner of any unclaimed Prize, if any, will be notified in writing by email within two (2) business days of the relevant draw and details of the winner of any unclaimed Prize will be published on the Promotion Website on the dates outlined in the table below.
23.	If for any reason this Promotion is interfered with in any way or is not capable of running as planned due to any reason beyond the reasonable control of the Promoter, including but not limited to technical difficulties, unauthorised intervention or fraud, the Promoter reserves the right in its discretion, to the fullest extent permitted by law to: (a) modify suspend, terminate or cancel the Promotion as appropriate, subject to approval of the gaming authorities in each State and Territory where relevant; (b) disqualify any entrant.
26.	Nothing in these Conditions of Entry limits, excludes or modifies or purports to limit, exclude or modify the statutory consumer guarantees as provided under the Competition and Consumer Act, as well as any other implied warranties under the ASIC Act or similar consumer protection laws in the States and Territories of Australia ("*Non-Excludable Guarantees*"). Except for any liability that cannot by law be excluded, including the Non-Excludable Guarantees, the Promoter (including its respective officers, employees and agents) excludes all liability (including negligence), for any personal injury; or any loss or damage (including loss of opportunity); whether direct, indirect, special or consequential, arising in any way out of the Promotion.


Renowned designer Holly Hollenbeck of HSH Interiors undertook an extensive renovation, delightfully blending bright colors and bold patterns with the timeless architecture.
The 5,745-square-foot manor has been vibrantly rejuvenated for stylish modern living while retaining stately classic elements, including decorative stained-glass windows, carefully refinished oak floors, and regal moldings, paneling, and staircase railings.
The formal living space encompasses an inviting sitting area and a more classical room with herringbone-patterned solid-oak floors, a fireplace, and views of the park.
The refined formal dining room includes a built-in buffet, a coffered ceiling, and handsome paneled walls.
The kitchen features a delightful combination of old and new, with a stained-glass window, white Carrara marble countertops, and stainless-steel appliances.
The breakfast room features a vintage china cabinet with decorative leaded glass, a period fireplace with eye-catching tilework, windows that fill the space with light.
A grand central staircase with distinctive lighting and a colorful stained-glass window rises to the second level and the three restful bedrooms.
The master suite features a fireplace, built-in bookshelves, an enchanting vista, and an expansive walk-in closet and dressing area.
The en suite bath boasts striking custom tilework, a marble-clad shower, and a freestanding soaking tub overlooking the park.
A second stairway leads to the third level, which includes three bedrooms, a bath, an office and playroom, and a library with built-in bookshelves.
The home's lowest level includes a generous laundry area, welcome storage, and a flexible space capable of serving a variety of functions. A sunken terrace ideal for alfresco grilling, relaxing, or celebrating and an Astroturfed play area are secluded on the rear of the home.
The city's celebrated "Painted Ladies" are nearby, and Alamo Square Park, just across the street, is an enduring San Francisco landmark.


Watch Friday After Next (2002) : Full Movie Online Free Craig and Day Day have finally moved out of their parents houses and into their own crib. The cousins work nights at a local mall as security guards. When their house is robbed on Christmas Eve they team up to track him down.


text:
Young Security Man Becomes CEO of His Own Oil And Gas Company
by Maverick
AD Patrickson, as he said, worked hard from being a night watchman on oil vessels to being the CEO of an oil and gas company — not only did the story end there, as the young man himself said he had to bring a lot of hard work into his visionPatrickson said he was the first owner of a small downstream business in Cameroon without any professional assistance.
A young man has shared his inspirational success story about how he became an oil and gas company owner years after serving on oilfield vessels as a night-watchman.
The guy is known as AD Patrickson, and does not suggest something beats love and hard work. Patrickson said he had to pour in all of his to fulfill his vision.
He added that passion, he even helped his academics improve. Never to be one who doesn't give back, the downstream specialist said that while pursuing his career goal, he also contributed to his country, Cameroon. Now that he has paid off his debt, he is the CEO of Source Rock, the first local Cameroonian firm to "run a natural gas plant without specialist assistance."
Patrickson was on the left as he was starting out. He is seated on the bottom, as his company's CEO. He inspired any dreamer like him in his final words on his LinkedIn message, telling them never to give up, that the target is nearer than they thought. Briefly.co.za published in similar news about a local young woman, who also works with big dreams as an example to others. BusiswaLutshaba is a vibrant young woman born and raised in South Africa's third-largest informal settlement -Khayelitsha, Cape Town.
Her company interest and culture led her to found her own venture, called Blu Space Communications SA. The company is one based on public relations and aims to bridge the gap between young local entrepreneurs and governmental as well as corporate entities. Busiswa was appointed as the first social entrepreneur of the Unboxed Incubator System through the assistance of Soapbox.
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