text:
\section{Introduction to the CHANG-ES Survey}

\subsection{Motivation}
CHANG-ES (Continuum Halos in Nearby Galaxies---an EVLA Survey) is a project to  observe 35 edge-on galaxies in the radio continuum with wide bandwidths centred at 1.6 GHz (L-band) and 6.0 GHz (C-band,  using the Karl J. Jansky Very Large Array (hereafter, the VLA, formerly the Expanded Very Large Array or EVLA).  The wide bandwidths, $\Delta\,\upnu$, of the VLA (Table~\ref{tab:overview}) have made such a survey feasible since the theoretical signal-to-noise (S/N) improves as $1/\sqrt{\Delta \upnu}$, all else being equal.  For CHANG-ES, this has meant an order of magnitude improvement, on average, compared to any similar survey.   For example, \cite{hum91} achieved sensitivities ranging from 80 to 130 $\upmu$Jy beam$^{-1}$ rms and \cite{irw99} achieved 45 to 90 $\upmu$Jy beam$^{-1}$  rms at 5 GHz.  By contrast, typical rms values of the CHANG-ES D-configuration images are $\approx~6~\upmu$Jy beam$^{-1}$ at the same frequency (range of values for all configurations and frequencies are summarized in Table~\ref{tab:overview}).
Additionally, no previous survey has included polarization. This has opened up the possibility of exploring the magnetic fields in galaxy disks and halos for a well-defined galaxy sample.

{\renewcommand{\arraystretch}{1.1}
\begin{deluxetable}{lcc}
 \tabletypesize{\scriptsize}
\tablecaption{Overview of galaxy and observing parameters over frequencies and VLA
  array configurations.}
\tablewidth{0pt}
\tablehead{\colhead{\textbf{Parameter}}	           & \colhead{\textbf{Value}}	      & \colhead{\textbf{Ref}}}
\startdata
Galaxy Distance range                 &  4.4$\,\rightarrow\,$42  Mpc        & \cite{IV}\\
Galaxy SFR range                      &  0.02$\,\rightarrow\,$7.29 $M_\odot$/yr       &\cite{IV}\\
Galaxy optical diameter range          &  3.9$\,\rightarrow\,$15.8 arcmin  & \cite{I}\\
Array configurations (L-band, C-band) &  B C D, C D              & \cite{IV}\\
$\nu_0$ (L-band, C-band)	   & 1.58, 6.00 GHz			         & \cite{IV}\\
$\Delta\,\nu$ (L-band, C-band) & 512 MHz, 2.0 GHz		         & \cite{IV}\\
No. of spectral channels  (L-band, C-band) & 2048, 1024          & \cite{IV}\\
\vspace{0.1 in}
Approx. Spatial resolution range & 3$\rightarrow\,$60 arcsec  & \cite{XX,XXI,IV} \\
Typical resolutions in arcsec & & \cite{XX,XXI,IV}\\
(high-res, low-res uv weightings):&\\
~~~~~B configuration L-band  & 3, 6\\
~~~~~C configuration C-band  & 3, 6\\
~~~~~C configuration L-band  & 10, 15    \\
~~~~~D configuration C-band  & 10, 15   \\
~~~~~D configuration L-band  & 35, 45    \\
Approx. rms range& &\\
~~~~~(all configurations and bands)  & 3$\rightarrow\,$ 95 $\upmu$Jy/beam   & \\
\label{tab:overview}
\enddata
\end{deluxetable}

}

Wide bandwidths, when broken up into many individual channels, also provide advantages other than improved S/N: (a) radio frequency interference (RFI) can be more readily identified and excised, (b) {\it in-band} spectral index maps can be formed (e.g., Section~\ref{sec:TDE}), (c) Rotation Measure (RM) analysis can be carried out (Sections~\ref{sec:reversing} and \ref{sec25}), and (d) imaging can make use of the power of multi-frequency~synthesis.

CHANG-ES has a variety of goals. We wanted to understand the incidence of radio halos in `normal' spiral galaxies, determine their scale heights and correlate these results with other properties such as the underlying star formation rate (SFR) or SFR `surface density' (SFR per unit area, SFR$_{\rm SA}$). Measurements of outflow speeds can help to determine whether galaxies are more likely to experience winds or `fountain' flow.  Outflows in nearby galaxies could also represent low-energy analogues of the `feedback' that appears to be required in galaxy formation scenarios in order to control the star formation rate \citep{sil12}.  Since outflows can be observed with spectacular resolution in nearby galaxies, the physics of such systems may provide meaningful constraints on galaxy formation in the early universe. A consistent galaxy sample, with complementary data at other wavelengths, can also help us explore pressure balance in the ISM.  For more information on our science goals, see \cite{I}.

As indicated above, unique to the survey is that all polarization products were measured, namely Stokes I, Q, U, and V.  With analysis of linear polarization ($P\,=\,\sqrt{Q^2+U^2}$), along with RMs, an~in-depth understanding of the magnetic fields in these galaxies can be obtained, and several examples (Section~\ref{sec25}) have been very illuminating in this regard. Some of our galaxies show lagging halos (e.g., see others \citep[][]{zsc15}) either in optical emission lines or HI.  The reason for such lags is not yet understood, but an association with magnetic fields is possible \citep{hen16}.

A survey size that samples a sufficient number of galaxies in a reasonable (but large) total observing time resulted in 35 galaxies in total.  Clearly, rms values that improve upon previous measurements were desired. Since vertical features in galaxies show structures on virtually all scales, we required observations over a range of VLA array configurations. Thus, we have observed at B, C, and D-configurations in L-band and in C and D-configurations in C-band.  This also provides us with matching resolution for spectral index maps which are essential in understanding the origin of the emission (e.g., thermal or non-thermal fractions) as well as the propagation of cosmic ray electrons~(CREs).

Our galaxy selection criteria were (1) an inclination $>\,75^{\circ}$ as given in the Nearby Galaxies Catalog \citep{tul88} in order to easily see a halo,  (2) a declination  $>\,-23^{\circ}$ for detectability at the VLA, (3)~an optical size between 4 and 15 arcmin for a good match to the array configurations, and (4) flux densities at L-band of at least 23 mJy in order for a detection to be more likely.  Two more galaxies were added that did not meet these criteria but were included  because of other interesting known halo properties (NGC~5775 which was smaller than the lower angular size limit, and NGC~4244 which had a flux density below the minimum cut-off).

Notice that selection effects should be minor, the main one being the possibility that, by adopting a radio flux density limit, we could inadvertently be choosing galaxies with high SFRs.  However,~Table~\ref{tab:overview} reveals that our SFR range is quite typical of `normal' spirals. We do {\it not} choose our galaxies based on whether or not they have halos (except for the two mentioned above) nor do we specifically choose any active galactic nuclei (AGNs) although several were found to be present once the sample was defined.
Table~\ref{tab:overview} provides a summary of our data.  In all, over 405 hours of VLA time were granted for this large project.

\subsection{Techniques and Data Products}
\label{sec:techniques}

Data reduction was carried out using the Common Astronomy Software Applications (CASA) package\footnote{\url{http://casa.nrao.edu}}.  This allowed us to take advantage of a number of sophisticated imaging algorithms such as multi-scale multi-frequency synthesis (ms-mfs, \cite{rau11}).  `Multi-scale' assumes that any intensity feature can be represented by spatial scales of varying width prior to convolution with the synthesized beam, as opposed to the traditional assumption that an intensity feature is represented as a series of points.  `Multi-frequency' employs the technique of sampling differing spatial scales as the frequency varies across the band, thereby more thoroughly filling in the uv plane.  In addition, these techniques, as employed in CASA, allow for the fitting of in-band spectral indices across any individual band. In~principle, one can solve for curvature, $\beta$, in the spectral index as well  (i.e., $I_\nu\,\propto\,\nu^{\alpha+\beta log\nu}$ but our tests showed that the S/N for any given data set was not high enough to take advantage of the curvature option \citep{II}.  Hence, a straight line in log space  ($\beta\,=\,0$) was fitted across the band while imaging.  Thus,~a solution for the  in-band spectral index, $\alpha$, was obtained point-by-point, in each galaxy.

At the time of writing, D-configuration images \citep{IV} have been released at our data release website\footnote{\url{https://www.queensu.ca/changes}}, the B-configuration images have also been released \citep{XX} and the C-configuration \citep{XXI} data release is imminent.  Release data include total intensity images at two different uv weightings,  i.e., `robust 0' and `robust 0 + uv taper', specified as high-res and low-res, respectively, in~Table~\ref{tab:overview}. Both~non-primary-beam-corrected and primary-beam-corrected versions are included. At~D-configuration, linear polarization and polarization angle maps, and in-band spectral index maps are also available.  At~high resolution, where emission is weaker, we opted to include band-to-band spectral index maps, rather than in-band spectral index maps, i.e.,  C-configuration C-band to B-configuration L-band $\alpha$ maps.

Because the largest angular size detectable at the VLA is 16 arcmin at L-band and 4 arcmin at C-band, it was necessary to supplement the VLA data with single-dish data for the largest galaxies at L-band and all galaxies at C-band (Table~\ref{tab:overview}).  This has been accomplished with over 200 h of supplementary Greenbank Telescope (GBT) observations.  Because the GBT wide-band instrumentation was delayed and because data reduction algorithms had to be developed, all GBT observations are completed but the data reduction is currently in progress.  For several galaxies (NGC~891, NGC~4565, and NGC~4631), Effelsberg data have been used for the large-scale total intensity emission.

Complementary to our radio data, we have obtained
H$\alpha$ images using the Apache Point Observatory 3.5-m telescope \citep{XVII} for 21 galaxies, supplemented with images from the literature for the remaining galaxies.  This data set was obtained to assist with the thermal/non-thermal separation analysis (Section~\ref{sec:therm_nontherm}) and will also soon be publicly released.  We also have WISE enhanced resolution images of all galaxies and XMM-Newton and Chandra data for a large fraction of the sample.

\section{CHANG-ES Highlights}

In the following sections, we review CHANG-ES results.  Rather than presenting the various papers in chronological order, we present the results topically.

\subsection{AGNs}
\unskip

As indicated in the introduction, we did not select AGNs in the CHANG-ES sample nor was the sample designed specifically for AGN detection.  However, galaxies with AGNs have turned out to provide some of the more interesting results to date, as follows.

\subsubsection{A Remarkable Nearby TDE: NGC~4845}
\label{sec:TDE}

Observations of NGC~4845 resulted in a serendipitous radio detection \citep{V} of a Tidal Disruption event (TDE) approximately one year after its hard X-ray outburst \citep{nik13}.  These authors attribute the X-ray variability to a super-Jupiter mass object being devoured by a $10^5~M_\odot$ black hole.  CHANG-ES detected the radio emission as well as the {\it variability} of the radio emission from its five independent data sets spanning approximately 6 months. Remarkably, this is a very close TDE since the galaxy is in the Virgo Cluster.

The power of in-band spectral fitting paid off for this strong source.  Because we had 3 total intensity data points at L-band, 2 total intensity points at C-band, as well as in-band spectral indices for each one of these data points, it was possible to fit a spectrum to the AGN.  As shown in Figure~\ref{fig:N4845}a, the AGN is a GHz-peaked source (GPS) which is an order of magnitude closer than any GPS source seen before.  The spectral peak both declines with time as well as shifts to lower frequencies.

\begin{figure*
\centering
\begin{tabular}{cc}
\includegraphics[width=4.8 cm]{N4845_spectrum-eps-converted-to.pdf}&
\includegraphics[width=7cm]{N4845_V-eps-converted-to.pdf}\\
({\bf a})&({\bf b})\\
\end{tabular}
\caption{The galaxy, NGC~4845. (\textbf{a}) {\bf Left:}  spectrum of the AGN in NGC~4845 from three different time steps, the earliest in red (T1), T1 + 56 days in green, and T1 + 196 days in blue, from \cite{V}. (\textbf{b}) {\bf Right:} Contours of Stokes V over total intensity image in colour at L-band, from \cite{XI}. The beam is shown at the lower left.}
\label{fig:N4845}
\end{figure*}

The low frequency turnover has been explained by synchrotron self-absorption and the behaviour of the emission modelled by adiabatic expansion of conical or jet-like outflow \citep{V}. Our model further predicts the rate of decline of the radio emission with time which is $S_\nu\,\propto\,t^{-5/3}$ for cone-like geometry (Equation (22) of \cite[][]{V}).   Follow-up observations 3 and 4 years later
show a good fit to the predicted $t^{-5/3}$ decline (\citep[][]{per17}, and additional as yet unpublished data).

The fact that such a nearby galaxy harbours a TDE-related outburst means that such systems can be monitored with unprecedented resolution. The relationship between classical AGNs and TDEs may simply be a matter of how much mass is involved in the infall and how sporadically the related outburst occurs.  A second TDE has now also been identified in NGC~660 in the X-ray.

\subsubsection{Circular Polarization}

Circular Polarization (CP) is a difficult quantity to measure in extragalactic sources since it is typically very weak (V/I $\approx$ 0.2\%) and is technically challenging.  Nevertheless, the TDE source, NGC~4845, shows a very strong CP signal of $\approx$ 2\% at L-band near the turnover to optical thickness in the spectrum \citep{V}. This unusual result prompted us to search through all of the galaxies at high resolution (B configuration L-band), resulting in three more detections (NGC~4388, NGC~660, NGC~3628) and~a marginal detection in NGC~3079 \citep{XI}. In all cases, the detection was right at the core of the galaxy. Weaker signals (less than approx.~$0.2$\%) could potentially be present in the sample but could not have been detected with our technical set-up.  The explanation that is most consistent with the data is {\it Faraday conversion} which converts linear to circular polarization along a line of sight (e.g., \citep[][]{ken98}).  The facts that no linear polarization is observed, that the Stokes V spectrum is very steep ($\alpha_V\,\approx\,-3$), and that CP is observed close to the optically thick limit, are in agreement with this interpretation.  We provide practical expressions for the Stokes V flux density for a variety of physical conditions in galaxy cores~(\citep[][]{XI}, Appendix A).  We also note that the two galaxies with the strongest 2\% signals are also those which have the most luminous X-ray cores.

Unlike previous measurements (with the exception of the Galactic Center), CHANG-ES has now revealed {\it nearby} galaxies with a CP signal, again providing clearer laboratories than before for studying such phenomena.   Such a study is only in its infancy but has the potential to reveal activity deep into the core where linear polarization is undetectable.  Never-before-seen-related phenomena have now been observed, for example, what we have called the `conversion disk' in NGC~4845 as seen in Figure~\ref{fig:N4845}b.  Here, Stokes V contours are shown over the total intensity emission at L-band, revealing a disk that is tilted with respect to the total intensity emission.  Presumably, the conversion disk has something to do with the shape of a linearly polarized signal prior to conversion.

\subsubsection{Hidden AGN-Related Activity Revealed}

The polarization capability of CHANG-ES has revealed previously hidden AGN activity which had either been masked or was not as clear in total intensity.  A good example is NGC~2992, whose~bipolar radio structure is only revealed in polarization \citep{VIII}.  NGC~3079 is another galaxy whose radio lobes are more clearly seen in polarization.

Hidden AGN-related activity can also sometimes be revealed via the spectral index maps.  An~example is NGC~3628 which shows bipolar radio emission perpendicular to the major axis via flatter spectral indices in comparison to the surrounding emission \citep{XX}.

These results show the importance of both polarization and spectral index mapping in disentangling AGN-related emission from emission related to other processes.

\subsubsection{Frequency of AGNs}

For the CHANG-ES galaxies, like other spirals, it has historically been a challenge to understand whether outflows might be due to stellar winds and supernovae (SNe) (SF-related activity), or whether the outflow is due to AGNs.  This is because there could very well be both types of activity in galaxy nuclei.  Theoretically, we expect supermassive black holes to be present in all galaxies (e.g., \citep[][]{kin16}), although this does not necessarily imply AGN activity.  Additionally, low-luminosity AGNs (LLAGNs), when~present, can be `buried' in other types of emission.

Since the CHANG-ES galaxies are edge-on, obscuration can be severe at other wavelengths so adopting radio criteria for AGNs is useful.  We use (1) the presence of point-like cores, (2) a luminosity that is too high for a collection of SNe, (3) flat or positive spectral indices at the centre, (4) the presence of bipolar or lobe-like structures, (5) time variability, and (6) CP.  Using these criteria where possible, we find an occurrence of 55\% of the sample \citep{XX}. This is a lower limit because weak LLAGNs could still be present in some cases and missed by our criteria.  Higher resolution observations in the future would help to further distinguish AGNs from central starbursts.

\begin{figure*}[ht]
\centering
\begin{tabular}{cc}
\includegraphics[width=7 cm]{scaleheight_diameter.jpg}&
\includegraphics[width=7 cm]{normalizedheight_massdensity-eps-converted-to.pdf}\\
 ({\bf a})&({\bf b})\\
 \end{tabular}
\caption{Galaxy-scale height correlations from \cite{IX}. ({\bf a}) {\bf Left:} Scale heights increase with the radio diameter of the galaxy.  ({\bf b}) {\bf Right:} Normalized scale heights {\it decrease} with the mass surface density of the underlying disk.}\label{fig:scaleheights}
\end{figure*}

\begin{figure*}[!htb]
\centering
\includegraphics[width=10 cm]{finalHSTdiskMedianhalo.jpeg}
\caption{The median edge-on spiral galaxy (in blue-grey) in L-band made from stacking 30 of the CHANG-ES galaxies all scaled to the same angular size. The median image is superimposed on an optical Hubble Space Telescope image of NGC~5775. Modified from \cite{IV} by Jayanne English (NRAO/AUI/NSF; NASA/STScI).}
\label{fig:median}
\end{figure*}

\subsection{Edge-on Disks and Thermal/Nonthermal Separation}
\label{sec:therm_nontherm}

Since we would like to understand the propagation of CREs as a function of position in our galaxies, we need the non-thermal spectral index, $\alpha_{NT}$, as well as the spatially resolved thermal fraction in the CHANG-ES galaxies.  To assist with this, we have obtained H$\alpha$ maps of most of our galaxies, with the remainder taken from previously published data.  Since both thermal radio emission and H$\alpha$ emission are proportional to the emission measure, EM, the H$\alpha$ maps, corrected for dust, can~be used to predict the thermal fraction in the radio. The non-thermal emission can then be found as a function of position in the galaxy.

This issue has been addressed by others in the past
(e.g., \citep[][]{tab07,tab17}), but not specifically for edge-on galaxies for which dust extinction can be severe.  The first indication of this comes from \cite{VI} in a plot of L-band luminosity against SFR for the CHANG-ES galaxies, with the SFR determined from the 22 $\upmu$m luminosity.  This plot is essentially the mid-IR radio continuum relation for our galaxies and shows a normalization that differs from face-on systems.  That is, for a given radio continuum luminosity, the~SFR is {\it low} by a factor of two to three, suggesting that the 22 $\upmu$m flux may itself be suffering from some extinction.  Thus, standard corrections for dust need to be modified for edge-on or very dusty galaxies.

A variety of tests \citep{X} have shown that, for resolutions of typically 10 arcsec ($\approx 1$ kpc at 20 Mpc),
\begin{equation}\label{th_nonth}
L\left({\rm H}\alpha_{corr}\right)\,=\,L\left({\rm H}\alpha_{obs}\right)\,+\,0.042 \nu L_\nu\left(24\upmu{\rm m}\right)
\end{equation}
where $L$ is the luminosity, $corr$ and $obs$ refer to corrected and observed, respectively, and the $24~\upmu{\rm m}$ luminosity (approximately the same as at $22~\upmu$m) corrects for dust.  The constant is about 1.4 to 2 $\times$ larger than previous authors and takes the higher extinction into account.

It should be pointed out that in the highest resolution images (3 arcsec, or $\approx\,300$ pc at 20 Mpc), in which HII region complexes in disks start to be resolved, the thermal fraction can be higher than Equation~(\ref{th_nonth}) predicts when applied to those discrete HII regions \citep{XVII}.

\subsection{Vertical Scale Heights, Winds, and Some Unexpected Results}
\label{sec:scale_heights}

An important goal of the CHANG-ES survey is to measure vertical scale heights in our galaxies, an improvement over simply measuring the radio halo extent to some contour level since scale heights will not be strongly dependent on the sensitivity of the image.  Such information (e.g., the~ratio of scale heights at two frequencies) can tell us something about the way in which cosmic rays propagate away from the disk, e.g., via diffusion or winds, as outlined via the SPINNAKER code of \cite{hee16, hee18}. Careful~measurements are required, ensuring that only the highest inclination galaxies and galaxies for which there are no missing large spatial scales are included in the sample. We have therefore measured scale heights in 13 galaxies \citep{IX} finding sample averages of $1.4\,\pm\,0.7$ kpc at L-band and $1.1\,\pm\,0.3$ kpc at C-band.

An unexpected result is that, when scale heights are correlated with a variety of parameters (e.g.,~SFR, B-field strength, etc.), the strongest correlation is actually with galaxy {\it size}, i.e., larger galaxies have larger radio halos (see Figure~\ref{fig:scaleheights}a).  Further analysis suggests a good correlation with global SFR~\cite{XVII}.
The physical reason for this correlation and its relation to star formation is discussed in Krause (2019, this volume).

If we remove the dependence on size by forming a {\it normalized} scale height scale, we now see an {\it inverse} dependence of the normalized scale height on underlying mass surface density (Figure~\ref{fig:scaleheights}b). That is, as the underlying surface mass increases, the normalized scale heights decrease.  This is the first evidence for gravitational deceleration in vertical outflows. Subsequent observations~(e.g., NGC~4666~\citep[][]{XIII}) agree with this result.

Once the normalized scale heights are considered, SPINNAKER results show that outflow velocities are consistent with galactic winds with speeds exceeding the escape velocity of the galaxy.  Again, subsequent observations \citep[][]{XII,XIII,XV,XVI} agree with this.

A beautiful illustration of global halos can also be seen in
Figure~\ref{fig:median} in which we show the `median edge-on galaxy' in total intensity modified from \cite{IV}. Thirty galaxies have been scaled to the angular size of the largest galaxy, the median formed, and then superimposed on an optical scaled image of the galaxy, NGC~5775.

\subsection{Magnetic Fields and their Orientation---Reversing Fields}
\label{sec:reversing}

\begin{figure*}[!ht]
\centering
\includegraphics[width=12 cm]{N4631_RMreversals-eps-converted-to.pdf}
\caption{Total intensity emission contours over a colour image of RMs in NGC~4631 from \cite{XIV}. Linear polarization vectors corrected for Faraday rotation are shown in red. Notice the east/west positive/negative RM reversals in the halo to the north of the disk.  The colour scale at top specifies the RM values.  The beam is shown as a red dot at the lower left.}
\label{fig:n4631}
\end{figure*}

One of the most remarkable results from the CHANG-ES survey is the discovery of {\it reversing magnetic fields} in our galaxy disks and halos.  Such a careful and detailed look at halo magnetic fields has never before been carried out and is assisted by the application of the Rotation Measure Synthesis (RMS) technique \citep{bre05}. A number of CHANG-ES galaxies have now had their magnetic fields probed using this technique (e.g., Section \ref{sec25} below).

The most stunning result can be seen in NGC~4631 (Figure~\ref{fig:n4631}) which has a well-known strong halo.  Here, we see systematic reversals  (positive/negative) in the RM (implying systematic reversals in the magnetic field direction) in the halo of the galaxy on kpc scales.  This is the first time that such a regular pattern has been seen in any galaxy halo.
Follow-up modeling of NGC~4631 by~\cite{woo19} and earlier papers~\citep{hen18a, hen18b}  have shown that such fields follow from scale-invariant or self-similar solutions of the classical dynamo equations.
The amplitude of these fields is constant on cones in the halo and disc
but the field lines are not confined to these cones. Rather, the field lines  have quite general poloidal components that frequently loop over the spiral arm projections for the asymmetric modes. The axially symmetric mode also has spiral and poloidal projections.  This structure remains a prediction to be tested. However, such field geometry is compatible with the existing observations in CHANG-ES~galaxies.

 Sign reversals in edge-on disks have now also been observed \citep{XIII} as well as in other CHANG-ES galaxies (not yet published).

\subsection{Individual Galaxies} \label{sec25}

In this section, we focus on some individual galaxies that have received attention from the CHANG-ES consortium so far.  They were studied in some detail for a variety of reasons, some of which are related to the PhD programs of our student members.

\subsubsection{UGC~10288}

\begin{figure*}[!ht]
\centering
\includegraphics[width=10cm,height=5cm]{UGC10288-eps-converted-to.pdf}
\caption{UGC~10288 after combining all data sets, resulting in a central frequency between L-band and C-band (4.1 GHz). The strong vertical feature near the centre is a background double-lobed source. The beam (not shown) is 6.5 arcsec in size.}
\label{fig:u10288}
\end{figure*}

UGC~10288 (Figure~\ref{fig:u10288}) was studied in some detail early in the project \citep{III}.  For this galaxy, we~combined all five total intensity data sets to obtain a single image at a frequency intermediate between L-band and C-band (4.1 GHz).  The fact that in-band spectral index fitting occurred at every position in the galaxy (Section~\ref{sec:techniques}) allowed such a combination to be carried out.

Surprisingly, most of the emission from the location of this galaxy is due to a bright background double-lobed radio source (`CHANG-ES A') whose central AGN is situated just above the disk of UGC~10288 and whose southern radio lobe shines right through the disk.  The radio emission from UGC~10288 itself would have fallen below our flux density limit for CHANG-ES, had the background galaxy flux density been subtracted off.  This result warns that care is required in interpreting discrete features that appear to be in the galaxy but may in fact be background sources, especially for such sensitive observations (see also \cite{XX}).

In spite of the corresponding downwards revision of the SFR for UGC~10288 ($\approx$0.4 $M_\odot$/yr), vertical discrete radio continuum features can still be seen extending out of the disk of this galaxy.  A~preliminary RM analysis of the light from the background source as it passes through the disk and halo region of UGC~10288 gave hints of RM reversals, though not with the stunning regularity shown for NGC~4631 in Figure~\ref{fig:n4631}.

\subsubsection{NGC~4666}

The CHANG-ES radio continuum data of the superwind and starburst galaxy NGC~4666 (Figure~\ref{fig:n4666} and \cite{XIII}) show a boxy radio halo in total intensity as well as in the X-ray.  The wind is likely driven by supernovae across almost the entire disk.
For the first time, the central point source was observed at radio
wavelengths. In our X-ray data, clear AGN fingerprints were detected, which supports previous findings from X-ray observations that NGC 4666 harbors an AGN.

\begin{figure*}[h]
\centering
\includegraphics[width=11 cm]{N4666_CC_bw_features_con_neu-eps-converted-to.pdf}
\caption{C-band image of NGC~4666 in gray scale and contours, the latter at 0.22, 0.44, and 0.88 mJy beam$^{-1}$ with a beam (shown at the lower left) of 3.0$^{\prime\prime}$~$\times$~3.5$^{\prime\prime}$. The central contour depicts the AGN in this galaxy and other features are labelled.  From \cite{XIII}.}
\label{fig:n4666}
\end{figure*}

The high resolution combined C-band data of NGC 4666 (Figure~\ref{fig:n4666}) show remarkable filamentary vertical structures reaching into the halo-like fingers.
A scale height analysis reveals
a thick disk with a mean scale height of 1.57~$\pm$~0.21  kpc (C-band) and 2.16~$\pm$~0.36 kpc (L-band). The CR transport was modelled with the SPINNAKER code and found to have an advective wind
of
310 km~s$^{-1}$. This is different from the CHANG-ES galaxy NGC~4013 \citep{XIX}, where diffusion seems to be the dominant CR transport process.

NGC 4666 is characterized by an extended X-shaped structure with magnetic field vectors reaching far into the halo.
The mean disk magnetic field strength is 12.3 $\upmu$G, which is in good agreement with the field strength of other spiral galaxies \citep{bec16}.
The analysis of the C-band RM-synthesis map along the major axis of NGC~4666 shows indication of one disk magnetic field reversal at a radius of 30" (4 kpc). The field orientation is likely axisymmetric and points inwards and then outwards with increasing radial distance
from the centre (please see \cite{XIII} for more details on the analysis). This is the first time that an indication of
a radial field reversal within the disk is observed in an external
galaxy. As we saw for the magnetic field reversals in the halo of NGC~4631 (Section~\ref{sec:reversing}), these findings are consistent with mean-field dynamo theory (e.g., \cite[][]{moss2012}).

\subsubsection{NGC~4388}

In the case of this Virgo galaxy, the sensitivity provided by the use of the RM-synthesis technique on our C band-C configuration data \citep{VII} was key to revealing a large number of new faint features in the halo (Figure \ref{fig:n4388}). With an exceptionally low rms noise of 2.3 $\upmu$Jy/beam and a resolution of 5.33 arcsec in polarized intensity, we are also able to resolve some interesting features of the disk never seen before.
\begin{figure*}[h]
\centering
\includegraphics[width=11 cm]{NGC4388_Pol.pdf}
\caption{Linearly polarized intensity at 6 GHz in contours plus magnetic vectors corrected for Faraday rotation, with a resolution of 5.33 $\times$ 5.33 arcsec and an rms noise of 2.3 $\upmu$Jy $\rm{beam}^{-1}$. The contour levels are (3, 5, 8, 16, 32, 64, 128) $\times$ 2.3 mJy $\rm{beam}^{-1}$.  The beam is shown as a white dot at the lower left.}
\label{fig:n4388}
\end{figure*}

This is a Seyfert 2 galaxy with many processes occurring at the same time. There are several outflow events detected at different wavelengths (i.e., H$\alpha$, X-ray, HI) whose kinematics and morphology are strongly modified by the strong ram-pressure action of the intracluster medium (ICM). The brightest emission in radio polarization in our VLA map is detected at the northern part of the nuclear outflow, where the magnetic field vectors are oriented along the outflow structure. Our data also show for the first time a well defined southern nuclear outflow where the magnetic field vectors are distributed in an S-shaped structure, which is an indication of a connection between the bright radio spots detected above the disk and the nucleus of the galaxy. The halo also shows two polarization filaments to the north and south of the nuclear outflow that extend up to $\sim 5~\rm{kpc}$ in the case of the northern filament. These structures seem to also be connected to the nuclear activity due to its symmetry with respect to the centre. It is still unclear whether their origin is AGN- or star formation-related.

NGC~4388 shows two extended blobs of polarized signal towards the southeast and the northwest parts of the halo and their magnetic field vectors are oriented perpendicular to the disk of the galaxy. By computing the half-life time of the CREs in these regions, we can estimate how far into the halo these particles can reach before losing all their energy. We found that in order to reach heights between $2.9$ and $\sim 3.7\,\rm{kpc}$, they would need to travel at a speed of $270\,\rm{km~s^{-1}}$, which is typical for a galactic~win
.

\subsubsection{NGC~3556 and LOFAR Data}

Total power results from CHANG-ES observations of NGC~3556 were combined with results from 144~MHz observations carried out using the Low Frequency Array (LOFAR) \cite{XII}. These data were taken as part of the LOFAR Two-metre Sky Survey (LoTSS) \cite{LoTSS}. The combined results were used to calculate the spectral index between L-band and 144~MHz and the magnetic field strength in the galaxy using the equipartition approach by \cite{bec05}. This showed that the disk of the galaxy has an average magnetic field strength of 9~$\upmu$G, decreasing to around 5~$\upmu$G towards the halo. The magnetic field strength map is presented in Figure \ref{fig:n3556_bmap}.

\begin{figure*}[!ht]
\centering
\includegraphics[width=10 cm]{N3556_Lhba_B.png}
\caption{Magnetic field strength map of NGC~3556 derived through the equipartition assumption using the spectral index between $L$ band and $144$~MHz and synchrotron flux density at $144$~MHz. Red contours show the surface brightness distribution of the $144$~MHz map.  The beam is shown as a red dot at the lower left.}
\label{fig:n3556_bmap}
\end{figure*}

The total power values and the magnetic field strength were used to model the cosmic ray electron propagation using SPINNAKER \citep{hee16} and its interactive wrapper SPINTERACTIVE \footnote{\url{https://github.com/vheesen/Spinnaker}}. Multiple models of diffusive and advective propagation were tested. The best fitting result was an advective transport of the CREs with a linearly increasing wind speed.

\subsubsection{NGC~891 and NGC~4565}
The two nearby spiral galaxies, NGC~891 and NGC~4565, differ largely in their detectable halo extent and their star formation rates. The question is how these differences are related to the (advective and/or diffusive) CRE transport in the disk and halo. In C-band, the total power emission of both galaxies has been corrected for missing zero spacing flux with the single-dish 100-m Effelsberg telescope. After subtracting off the thermal emission, maps of the total magnetic field strength and the nonthermal spectral indices as well as vertical nonthermal scale heights at different radii could be determined \citep{XVI}.

These quantities were used to model the CRE transport by SPINNAKER. \citet{XVI} found that the CRE transport in the halo of NGC~891 is probably dominated by advection with an accelerated galactic wind reaching escape velocity at a height of 9 to 17 kpc. This wind is likely to coexist with diffusion-dominated regions. For NGC~4565, however, the halo is diffusion-dominated up to a height of at least 1~kpc with a diffusion coefficient being only weakly energy dependent.

The high-resolution total intensity radio map of NGC~4565 in C-band has a linear resolution of about 200~pc that allows the possibility of separating both sides of the large radio ring (which could also represent tightly wound inner spiral arms) in the disk, as shown in Figure~\ref{fig:n4565}. This ring-like feature must be very thin with a vertical thickness of only $260 \pm 100$~pc and horizontal width of $2.2 \pm 2.2$~kpc.

\begin{figure*}[h]
\centering
\includegraphics[width=11cm]{Fig4dN4565.jpg}
\caption{The galaxy, NGC~4565, in total intensity at C-band and resolution of 200 pc, zooming in on the large, thin, ring or inner spiral arms.  From \cite{XVI}. Notice the point-like core at the centre.  The beam is shown as a small black dot at the lower right.}
\label{fig:n4565}
\end{figure*}

\section{Conclusions}

The CHANG-ES sample of 35 edge-on galaxies has been observed in wide bands centred at 1.6 and 6.0 GHz over a variety of VLA array configurations.  This survey, which includes spatially resolved polarization and spectral index information, is providing new insight into the halo and disk-halo activity in spiral galaxies.

With thermal/non-thermal separation of the emission, measurements of scale-heights, and the sophisticated modeling of CRE outflows, the physical conditions in such regions are being probed in considerably more detail than ever before.  The results of such modeling suggest that most of our galaxies are experiencing outflowing winds.

AGNs have been revealed in the CHANG-ES sample in a variety of ways, including in circular polarization. Bipolar features can be seen in polarization or spectral index structures which otherwise have been masked in total intensity.

The polarization data together with a rotation measure synthesis analysis have now revealed structures that have never before been seen in any galaxy.  These are regularly reversing magnetic fields on kpc scales both in the disk and halo, likely because of magnetic dynamo action.

We summarize CHANG-ES papers to date in Table~\ref{tab:listofpapers}. CHANG-ES FITS images are available at the data release web site:
\url{https://www.queensu.ca/changes}.

\begin{landscape}
{\renewcommand{\arraystretch}{1.1}
\begin{deluxetable}{lc}
 \tabletypesize{\scriptsize}
 \tablecaption{List of CHANG-ES papers to date.}
 \tablewidth{0pt}

 \tablehead{
   \colhead{\bf{Paper Title}}      & \colhead{\bf Ref}
 }
\startdata
CHANG-ES I: Continuum Halos in Nearby Galaxies: An EVLA Survey: Introduction to the Survey & \cite{I}\\
CHANG-ES II: Continuum Halos in Nearby Galaxies: An EVLA Survey: First Results on NGC 4631 & \cite{II}\\
CHANG-ES III: UGC 10288—An Edge-on Galaxy with a Background Double-lobed Radio Source & \cite{III}\\
CHANG-ES IV: Radio continuum emission of 35 edge-on galaxies observed with the \\
~~~~~~~~~~~~~~~~~~~~~~~~~~~~~Karl G. Jansky Very Large Array in D-configuration — Data Release 1 & \cite{IV}\\
CHANG-ES V: Nuclear Outflow in a Virgo Cluster Spiral after a Tidal Disruption Event & \cite{V}\\
CHANG-ES VI: Probing Supernova energy deposition in spiral galaxies through Multiwavelength\\
~~~~~~~~~~~~~~~~~~~~~~~~~~~~~relationships & \cite{VI}\\
CHANG-ES VII: Magnetic Outflows from the Virgo Cluster Galaxy NGC 4388&\cite{VII}\\
CHANG-ES VIII: Uncovering Hidden AGN activity in radio polarization & \cite{VIII}\\
CHANG-ES IX: Radio scale heights and scale lengths of a consistent sample of 13 spiral galaxies\\
~~~~~~~~~~~~~~~~~~~~~~~~~~~~~seen edge-on and their correlations & \cite{IX}\\
CHANG-ES X: Spatially Resolved Separation of Thermal Contribution from Radio Continuum\\
~~~~~~~~~~~~~~~~~~~~~~~~~~~~~Emission in Edge-on Galaxies & \cite{X}\\
CHANG-ES XI: Circular polarization in the cores of nearby galaxies & \cite{XI}\\
CHANG-ES XII: A LOFAR and VLA View of the Edge-on Star Forming Galaxy, NGC 3556 & \cite{XII}\\
CHANG-ES XIII: Transport processes and the Magnetic Fields of NGC 4666 — Indication of a\\
~~~~~~~~~~~~~~~~~~~~~~~~~~~~~Reversing Disk Magnetic Field & \cite{XIII}\\
CHANG-ES XIV: Cosmic-ray Propagation and Magnetic Field Strengths in the Radio Halo of NGC~4631 & \cite{XIV}\\
CHANG-ES XV:  Large-scale Magnetic Field Reversals in the Radio Halo of NGC~4631& \cite{XV}\\
CHANG-ES XVI: An In-Depth View of the Cosmic-ray Transport in the Edge-on Spiral Galaxies\\
~~~~~~~~~~~~~~~~~~~~~~~~~~~~~NGC 891 and NGC 4565 & \cite{XVI}\\
CHANG-ES XVII: H-alpha Imaging of Nearby Edge-on Galaxies, New SFRs, and an Extreme\\
~~~~~~~~~~~~~~~~~~~~~~~~~~~~~Star Formation Region — Data Release 2 &\cite{XVII}\\
CHANG-ES XVIII: The CHANG-ES Survey and Selected Results & \cite{XVIII}\\
CHANG-ES XIX: The Galaxy NGC 4013 — A diffusion-dominated radio halo with plane-parallel&\\
~~~~~~~~~~~~~~~~~~~~~~~~~~~~~disk and vertical halo magnetic fields & \cite{XIX}\\
CHANG-ES XX: High Resolution Radio Continuum Images of Edge-on Galaxies and their AGNs\\
~~~~~~~~~~~~~~~~~~~~~~~~~~~~~— Data Release 3&\cite{XX}\\
CHANG-ES XXI: Radio continuum emission of 35 edge-on galaxies observed with the\\
~~~~~~~~~~~~~~~~~~~~~~~~~~~~~Karl G. Jansky Very Large Array in C-configuration — Data Release 4&\cite{XXI}\\
\enddata
\label{tab:listofpapers}
\end{deluxetable}
}

\end{landscape}

\vspace{6pt}

\acknowledgments{The first author wishes to thank the Natural Sciences and Engineering Research Council of Canada for a Discovery Grant.}

redpajama_set_name: RedPajamaArXiv


There some weird thing with this driver and ati mobility m6 in the HP nc4010. Zeta: screen switches to black after boot icons, BeOS with same? bebits driver too, solution: remove driver, reboot, reinstall, reboot works. In zeta select Use panel = always in screen prefs and your sceen won't go black after colour depth changes.
In haiku the 'remove driver, reboot, reinstall, reboot'-method won't work, screen stays black. With radeon driver from bebits this method works but I can't set sceen resolution or colour depth (it won't change anything).
IRQ is deactivated in Haiku Radeon driver (by axeld). To have it working along an audio driver (for the same IRQ IIRC), I had to activate IRQ again.
Where / how can I activate the IRQ for VGA? I'd like to test it. If I use the radeon driver from Bebits, should the screen prefs work? Do the screen prefereces work at all? There's like I said before an issue with the panel (screen) not being activated and thus the screen stays black, who maintains the driver?
Seems that the backlight isn't always activated with the bebits radeon driver (originally by Tomas Kurschel, now maintained by Euan). Could be related, see the bebits talkback if you have time.
This bug should have been fixed already, since interrupts have been reactivated for the radeon driver.
This bug still persists, I had to put an external monitor to the vga out to get a picture to be able to set the "Use laptop panel" "Always" After that it works.
This time a installed Haiku rev 18081 over the older version but didn't replace the settings folder in /boot/home/config/settings.
I cannot get the latest Radeon driver to work with Haiku (18203) at all with my Radeon 9200 AGP. I also have an SB Live Value! in this machine - if that matters.
I had to revert 17279 and rebuild the driver in order to successfully boot Haiku with it again.
I'm thinking this bug is closed now?
9200 bug was hrev20336 #1079 and the backlight issue was semi-solved for those lucky people shortly later?
I feel new tickets for those unlucky people would be easier for traceability, given the number of changes to the driver in the last 12 months. If anyone wishes to post a new ticket for backlight issues, can they post a syslog (with file name containing reporters name + laptop model). Everyone else just pile on more syslogs in a similar fashion.
If no objections I'll close this ticket.


text:
Park Regionalny Molentargius – Saline – jeden z parków regionalnych we Włoszech w pobliżu stolicy Sardynii – Cagliari. Powstał w 1999 roku.

Historia
Została ona założona w 1999 r. w celu ochrony i wzmocnienia miejsca o znaczeniu międzynarodowym, już objętego Konwencją Ramsar od 1977 r. ze względu na jego znaczenie związane z międzylądowania, zimowania i gniazdowania gatunków ptaków ptactwa wodnego.

Teren
Park jest terenem podmokłym rozciągającym się na powierzchni około 1600 hektarów, otoczonym zurbanizowanymi obszarami Cagliari i innych miast aglomeracji oraz nabrzeża plaży Poetto.

Zbiorniki wodne
Wyjątkowość tego obszaru jest obecność zbiorników zarówno słodkiej i słonej wody, oddzielone równiną charakteryzuje się przeważającą suchość o nazwie "Is Arenas". Obszary ze słodką wodą to stawy Bellarosa Minore i Perdalonga.

Fauna

Ptaki
Jest to jedno z najważniejszych miejsc w Europie dla niezwykłej liczby ptaków, które tu przebywają. Obecnie 177 spośród 330 gatunków ptaków Sardynii żyje w dorzeczu Molentargius – ponad jedna czwarta wszystkich europejskich gatunków ptaków, takich jak m.in. flamingi i czaple. Od roku 1850 do chwili obecnej w rejonie Molentargius odnotowano 230 gatunków ptaków należących do 53 rodzin.

Zwiedzanie
Aby zwiedzić park, można skorzystać z wypożyczalni rowerów przy wejściu do parku, wsiąść do jednego z minibusów elektrycznych w parku, wybrać się na wycieczkę łodzią przez kanały lub podążać ścieżkami spacerowymi w okolicy.

Galeria

Przypisy

Turystyka we Włoszech
Sardynia
Cagliari
Parki i ogrody we Włoszech

redpajama_set_name: RedPajamaWikipedia


text:
District Advisory Commissionmdhoward_rivcpk2019-12-31T11:58:31-08:00
The Park District Advisory Commission (DAC) was established by the Park District Board of Directors (Riverside County Board of Supervisors) on June 28, 1994. The purpose of the Commission is to advise and make recommendations to the Board concerning the planning, acquisition, development, and use of parks and open space in unincorporated portions of Riverside County.
Additionally, the Commission is to advise the Board on matters relating to the acquisition, development, maintenance, and promotion of regional recreation trails in the County, and matters relating to the conservation and propagation of fish and game in the County.
To apply for a vacant commissioner position, please contact the Board of Supervisor for your district.
The District Advisory Commission generally meets bi-monthly on the first Thursday of the following months: January, March, May, July, September and November. The agenda gives the meeting location. Occasionally the meeting date will change, and the agenda will reflect the new date.
Fish & Game Funding Request Application
To access archived agendas and minutes, please click here.
Mark F. Balys
First District – Supervisor Jeffries
Born and raised in Niagara Falls, New York Mr. Balys graduated from Orange Coast College in Costa Mesa, CA and from U.C. Riverside. After a 34 year career with the Riverside County Planning Department he retired as Deputy Planning Director. Since 1980 he has been on the Board of Directors of Altura Credit Union and is currently Vice-Chairman of the board. Mark has served Habitat for Humanity Riverside as a volunteer, board member, two-term past president, and most recently as Director of Fund Development. He and his wife Pam, a teacher at Matthew Gage Middle School, reside in Riverside. He was appointed to the Regional Park District Commission by Supervisor Bob Buster in 2010.
Amie Kinne
Amie Kinne was appointed to the Riverside County Regional Park and Open-Space District Advisory Commission on December 11, 2012. Ms. Kinne also serves as the Chair of the Riverside County Trails Committee. She grew up on the shores of Lake Superior in Northern Wisconsin. While being surrounded by vast open spaces and plenty of wildlife, her foundation of conservation and appreciation of nature was born. Ms. Kinne later moved to Southern California when she attended the University of California, Irvine. She has been actively reaching out to like-minded people as an equestrian, hiker, and photographer. She supports various conservancy groups, participates in clean ups, and has been involved with the Boy Scouts of America. Ms. Kinne enjoys reading field guidebooks and refers to herself as an amateur naturalist in training.
Second District – Supervisor Spiegel
Jon Christensen, originally appointed to the OHV Commission in 2010, was appointed to the OHVR Commission in February 2011 when it was formed under the Park District. Mr. Christensen was born and raised in Riverside County where his family settled and started farming in the 1880s. He spent nine years in the U.S. military, both in active duty and with the National Guard. He also volunteered for the U.S. Forest Service in the local Mountains. Mr. Christensen graduated from AMU with a degree in Management. He currently works for the County of Riverside's Treasurer Tax-Collector department as the Assistant Director where his daily operations include collecting 3 billion dollars of tax revenue and investing the County's 5.5 billion dollar AAA rated investment pool. Mr. Christensen, who is extremely active in the outdoors, enjoys hunting, camping, and riding motorcycles with his wife, two children, and son-in-law. He believes that OHV riding with his family has shaped his appreciation for our great outdoors and the recreational opportunities it provides.
Daniel Hake
Daniel Hake was appointed to the Riverside County Regional Park & Open Space District Advisory Commission in 2008. He previously served for six years as a member and chairman of the Riverside County Advisory Committee on Substance Abuse Programs. He retired in 2009 from the Orange County Sheriff's Department after 31-years of service and his educational background includes a Bachelor's degree in Criminal Justice and a Master's degree in Behavioral Science. Mr. Hake has resided in Riverside County for 30-years and enjoys participating in various outdoor actives with his family. He is also active in the community as a member and past president of the Rotary Club of Corona.
Robin Reid, Vice Chair
Third District – Supervisor Washington
Ms. Reid has been a resident of Riverside County for over four decades. Relocating from the Imperial Valley to the Palo Verde Valley, Robin grew up enjoying the outdoors with activities such as fishing, hunting, shooting, hiking and playing on the Colorado River. Robin and her husband enjoy hiking and off-roading with their dogs in the mountains and valleys surrounding the Hemet-San Jacinto Valley. She has a great love for the outdoors and appreciates thoughtful planning for recreation spaces and activities, as well as the preservation of natural habitats and open space. Ms. Reid has been a legislative and policy advisor in both the California State Legislature and the Riverside County Board of Supervisors. She holds an undergraduate degree in Social and Behavioral Science and attended California Southern Law School where she earned her Juris Doctor degree.
Anthony Migliore
Anthony Migliore was raised in Orange County and graduated from Cal-State Fullerton with a degree in International Marketing. He was accepted into the Naval Aviation Officer Candidate School in Pensacola Florida where he was commissioned as a Naval Officer and earned his wings. He earned his Masters Degree from the Naval Postgraduate School in Monterey California. After serving 21 years in numerous flying positions throughout the world, he retired from Naval service and settled with his family in the Temecula wine country. Mr. Migliore was a defense contractor and currently a General Contractor and partner in CLM Corporation. He is married to the former Susan Eaves of Sacramento and has three sons in College. His family enjoys County Parks and he is dedicated to developing and maintaining a wide spectrum of recreational areas in the County. He has served on Riverside County Commissions before serving as the 3rd District representative on the Parks and Open Space Commission.
Bob Grady, Chair
Fourth District – Supervisor Perez
Robert "Bob" Grady has been serving on the District Advisory Commission representing District IV and the Palo Verde Valley since 2005. He is a 36 year law enforcement veteran who retired as Chief of Police with the City of Blythe in 2004. He holds a degree in Public Service Management from the University of Redlands and an AA in Criminal Justice from Palo Verde College. He holds a California lifetime community college teaching credential. Mr.Grady also sits as Chair of the School Attendance Review Board with the Palo Verde Unified School District.
Daniel Hugh Van Horn
Daniel Hugh Van Horn, a longtime resident of Riverside County, was appointed as a District IV representative in July 2012. Hugh grew up in the Southwest part of the county and currently lives in Indio. He is the Branch Manager for International City Mortgage in Indian Wells, and also served as one of the co-chairs for the Temecula Valley Balloon and Wine Festival. Named one of Palm Springs 40 under 40 in the October issue of Palm Springs Life Magazine, Hugh is also on the Habitat for Humanity of Coachella Valley Family Selection Committee. In 2011, Hugh graduated from Leadership Coachella Valley, a program designed to identify, motivate and develop future community leaders. Prior to his career in the mortgage industry, Hugh performed in various theaters and them parks around Southern California including The Welk Resort, Disneyland, Legoland, South Bay Civic Light Opera, Musical Theater West, and Thousand Oaks Civic Arts Plaza, just to name a few. High and his wife Jeni have three young children and family is one of the most important things in his life. He believes that the Riverside County Regional park and Open-Space District provides a great service to its communities by providing places where families can share great moments and grow closer together.
Rick Croy
Fifth District – Supervisor Hewitt
Rick and his wife Kelley have lived in Southwest Riverside County for the past 20 years. As an avid equestrian, Rick has seen the rapid growth of the area and has a passion for presering all tail types which improve the overall quality of life for all resident.
Thomas Giedroyce
A retired printing industry professional with a Bachelor of Science degree from the Rochester Institute of Technology in Printing Management.
He has been involved in the city of Menifee since its incorporation in 2008 in a number of volunteer positions and activities. Including serving as Vice Chair of the city's Blue Ribbon Committee on Governance Structure. A member of the city's Menifee Citizen's Advisory Committee. And a member of the Menifee Parks, Recreation and Trails Commission which was created in 2014. While on the commission he has also served as its chairman and as its vice chairman.
He and his wife have been residents of Riverside County for over twenty years. They are avid horsemen who enjoy rural living and have bred, raised and trained show and pleasure horses.
Check out what RivCoParks has to offer:
The District preserves, protects, and provides services for over 70,000 acres of parks and open-space.
Families visit wild animals, live birds, snakes, and a variety of mammals entertaining and inspiring children.

redpajama_set_name: RedPajamaCommonCrawl


Based on a survey of more than 100 businesses and interviews with senior executives at 15 companies across a range of business sectors, the research found that many organisations are struggling to plan for the impact of digital on their business models and processes.
Marketing is the business function where there has been the biggest change over the past few years, with 86% of responding companies saying there has been a "huge impact" here. PR and communications has also changed radically, with 70% of respondents saying the impact has been major.
Other business functions where more than half of respondents say there has been a massive impact are customer service (59%), product and services development (58%), sales (57%) and market research (52%).
Linus Gregoriadis, Econsultancy's Research Director, said: "The way that sales and marketing functions have evolved over the last few years because of the internet is well documented. What has been less well explored is how companies can embrace digital technology and communications to improve other areas of their business such as HR and product development.
As well as carrying out an online survey of more than 100 businesses, Econsultancy and Blue Latitude interviewed senior executives, including CEOs and managing directors, at the following organisations: British Museum Company, Dell, Dyson, Dorling Kindersley, Electronic Arts, Glasses Direct, Kaplan, Ministry of Sound, 02, Penguin Books, Pentland Brands, Roche, Santander UK and Virgin Atlantic.


Patient Profile - The Fashion Flex is available for all ages, but recommended for adults. Fashion conscious patients or anyone who wants to wear high-heel shoes (2" high or greater) will find this device fitting for them. This device is designed for patients weighing 100-180 lbs.
Foot Type - The Fashion Flex is made to accommodate low to medium arch feet. This device is designed to maintain moderate midtarsal joint integrity for an elongated midstance, secondary to high-heel shoes.
Biomechanical Characteristics - The Fashion Flex is characterized by its narrowed forefoot, and the absence of any heel contour, which fitting it to high heel shoes easy and comfortable. The heel area is non-contouring (flattened) and is modified to match the pitch of the shoe.


text:
The women's team pursuit race of the 2015–16 ISU Speed Skating World Cup 1, arranged in the Olympic Oval, in Calgary, Alberta, Canada, was held on 14 November 2015.

The Dutch team won the race, while the Japanese team came second, and the Russian team came third.

Results
The race took place on Saturday, 14 November, in the afternoon session, scheduled at 15:07.

Note: NR = national record.

References

Women team pursuit
1


text:
HomeNewsCrimeIn the dock: Burgess Park paedo found guilty of abducting and sexually...
NewsCrimeIn the Dock
In the dock: Burgess Park paedo found guilty of abducting and sexually assaulting eight-year-old boy
By Court Reporter
Convicted: Shane Upton Photo credit: Central News
A homeless paedophile who kidnapped an eight-year-old boy from a park toilet and abused him in his woodland lair is facing years in jail.
Shane Upton, 24, sexually assaulted the terrified child in his makeshift tent as police frantically searched for the lad in Burgess Park, Walworth on June 17 this year.
The boy had been playing tennis with his brother as his mother looked on when he went to use the toilet a few yards away, Inner London Crown Court heard.
Jurors convicted Upton of kidnap, sexual assault on a child under 13, and two counts of causing a child to engage in sexual activity.
He was remanded in custody ahead of sentencing on January 6 next year.
Adrian Amer, prosecuting, said: 'The boy tells us that when he came out of a cubicle, he saw Shane Upton standing outside it.
"The man started talking to him and told him he was homeless and asked the boy to go to Southwark Housing with him so he could get a house.
"The boy said that the man locked in the entrance to the men's toilets and then locked the cubicle door.
"The complainant said that he tried to shout for help, but the man covered his mouth with his hands.
"He said that he felt scared and the man told him not to be scared.
Upton then performed sex acts on him, the court was told.
"He said this happened for a minute and then it stopped and he did it again," Mr Amer said.
Upton then took the boy out of the toilet's emergency exit.
He walked the boy around Burgess Park and a nearby housing estate for nearly an hour, before taking him to his tent.
"The boy said that the man told him that he lived in a tent and took him to a tent somewhere in Burgess Park," Mr Amer continued.
"The boy said that when they got in the tent the man went inside the tent and told him to come in.
"The boy said that he did not want to run away because he was scared and he knew that the man would catch him.
"He then describes going into a wooden cave made out of twigs and leaves. The man told him to lie down on his back.
"The man then pulled his trousers and pants down.
"The boy said that he was scared when this was happening so he closed his eyes because he wanted it to stop.
"He said that the man stopped when he realised the police were outside the tent.
"The boy said that the man ran off when he realised that the police were there. He said police chased the man and he then ran to the police officers.
"The boy said that he was very scared so he pulled up his pants and trousers and ran out of the cave.
"He said that the incident lasted about three to four minutes and that when he was in the tent he could hear a helicopter.
"Police on foot and on horseback and from a police helicopter conducted a search of the park,' said Mr Amer.
Police found Upton on top of the boy, with his jeans down below the waist committing a sexual act.
He was chased and caught when he fell over.
Upton, of no fixed address, denied but was convicted on the remaining counts of kidnap, one charge of sexual assault, one of committing an offence with the intent to commit a sexual crime and two of causing a child to engage in sexual activity.
The jury cleared Upton of two charges of assaulting an emergency worker and they earlier directed by the judge to clear him of a further count of sexual assault.
Burgess Park
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Jan Sidell 17th December 2019	At	11:45 pm
How terrifying for this little boy. Thank heavens his Mother was in the park with him. Now this paedophile had been found guilty lets hope the sentence he gets is commensurate with the offence. In other words Life Sentence. Because that's what he's given his 8 year old victim.
Mumzee British 28th January 2020	At	3:59 am
Why would you allow your 8 year old child to go to a public toilet by himself in this day and age?
#nonsense
usui je nye on 91-year-old former head


My favorite Italian duo, Lush & Simon, have whipped up another progressive masterpiece featuring wonder vocals from Delaney Jane. Their most recent release 'Hunter' ventured into different territory, shifting away from their melodic feel to a more aggressive sound. With 'In My Hands', the boys are back at the melodic having crafted another refreshingly uplifting, anthemic track with emotional vocals from Delaney Jane to boot. The song is set to be released on August 11th through Sander van Doorn's label, Doorn Records. For now, we have this rip from Tiesto's 'Club Life' to enjoy.
I currently reside in South Florida where Winter Music Conference in March is like Christmas. Catch me in Miami at Mansion, Story, or anywhere that showcases talented DJ/producers. I am a sucker for everything progressive house, am am drawn to top labels like Above & Beyond's Anjunabeats and Armin van Buuren's Armada. Favorite artists include those aforementioned, Audien, Tritonal, Zedd, Porter Robinson, Syn Cole, and Deadmau5.


text:
SBU News > Stony Brook Matters > University Enjoys Great Relationship With Wildlife Refuge
Stony Brook Matters
University Enjoys Great Relationship With Wildlife Refuge
As every Biology 101 student knows, symbiosis is a mutually beneficial relationship between two different entities. That's a good definition of the ties between the Quogue Wildlife Refuge and Stony Brook University.
Cara Fernandes '16
Two of the refuge's seven staff members are former Stony Brook students and the Refuge's employees have participated in the University's annual Earthstock celebration since 2012, educating Stony Brook students about Long Island's natural world and its inhabitants.
The refuge actively recruits its interns at Earthstock because of Stony Brook's focus on sustainability. The unpaid intern position is for 10 to 20 hours per week for a college student studying environmental, educational or animal-related sciences.
"Our experience with Stony Brook students has been great — they've always been excellent interns," says Assistant Director Marisa Nelson. "They are dedicated to their field of study, and luckily for us have knowledge about relevant environmental issues."
Some of Stony Brook's students have also found employment with the 305-acre non-profit nature preserve to be a perfect fit.
Cara Fernandes '16 of Baiting Hollow, New York, started at the refuge as an intern during summer 2014 as a co-educator for the Little Naturalist summer camp program.
These days she coordinates and teaches educational programs about Long Island's native plants, animals and ecology to a variety of audiences. She also cares for permanently injured wildlife, feeding them and administering medicine.
Her stewardship during her academic career at Stony Brook includes stints as president and secretary/event coordinator of the Long Island Water Environment Association, where she planned and executed events such as beach cleanups. As an eco-leader with the Office of Sustainability on campus, she participated in numerous recycling events and tree plantings. Cara also encouraged young students to pursue a career in marine and atmospheric science as a volunteer in the National Ocean Sciences Bowl Region Competition, the Bay Scallop Bowl, held on campus.
"Seeing so many students, faculty and professionals excited about the environment increased my interest in my career path, especially after attending the Indianapolis Prize nomination lunch for Carl Safina and Patricia Wright," says Cara.
Cara developed a love for the natural world because her father encouraged her sister and her to accompany him on hikes across Long Island.
What she most loves about her job at the refuge is teaching children and visitors about the environment.
Kimberly Stever '13
Kimberly Stever '13 of Rocky Point, New York, said that Stony Brook helped her embark on a meaningful career.
"My job at Quogue Wildlife Refuge was a happy accident. I had graduated from Stony Brook and was having trouble finding a position that suited my interests," Kimberly says.
She recommends that students contemplating careers in the environmental sciences take advantage of internships. "Many nature organizations on Long Island are small places and they remember people who put their time in there and care."
At the refuge, Kimberly maintains social media accounts, oversees catalog donations and assures that all donors receive proper acknowledgment. She also plans the Refuge's annual benefit gala, feeds and cares for animals, educates the public, and facilitates promotional planning and events. "The great thing about working here is that we all wear so many hats," she adds.
During the spring and fall, the refuge sends representatives to educate the public at fairs, including Earthstock, where Quogue Wildlife Refuge staffer Tony Valderrama appeared the last three years.
"We usually bring an animal based on specific conditions like the weather and the duration of the program we are featuring," Tony says. "From my experience people, love all animals but owls are a favorite, probably because they're so elusive but vocal in their nocturnal behavior.
"The interaction between the students and the wildlife is priceless," he adds. "My hope is that these simple interactions become a catalyst for future environmentalists. We are lucky to have the best interns every year who come from Stony Brook to work with us."
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text:
Formula 1: Fire accident – Grosjean reports from the fire hell
Grosjean reports on the hell of fire
Romain Grosjean survived a terrible fire accident at the Bahrain GP – also because a lot is being done for safety. Now he is reporting on it for the first time.
Romain Grosjean continues to recover from a serious fire accident in Riffa hospital. He has now spoken for the first time via an interview on French television.
"I saw that my visor was all orange and the flames were burning around me," said Grosjean in an interview with TF1. "Niki Lauda's accident came to mind. I didn't mean to end like this. I had to go out for my children. "
The Haas pilot continued: "I stayed in the flames for 28 seconds, but it felt a lot longer as I tried three times to get out of the cockpit. I was able to remove my seat belt. The steering wheel was no longer there. In the end my hands were burned and I had a huge sprain, thinking I broke my foot. After this accident, I am happy to be alive. "
He is now hoping to race again next week at the Abu Dhabi Grand Prix. "I was more afraid for my relatives, primarily my children, but also my father and mother," said Grosjean. "I wasn't really scared for myself. I saw death coming, I had no choice but to leave."
Grosjean compares his accident to Niki Lauda's
Niki Lauda's fire accident in 1976 at the Nürburgring is one of the most famous accidents in Formula 1 history. Probably also because the Austrian survived the accident. His burns on his face became a symbol of the Formula 1 era at that time. As world champion, Lauda united the glorious sides of the sport as well as the dangerous.
Four drivers were not so lucky and died in Formula 1 races because their cars went up in flames: Stuart Lewis-Evans at the 1958 Morocco GP, Lorenzo Bandini at the 1967 Monaco GP, Jo Schlesser at the 1968 French GP or Roger Williamson at the Dutch Grand Prix in 1973. Ronnie Peterson would have survived his fire accident in 1978, but died in hospital of an embolism.
Since then, various safety measures have ensured that fire accidents in Formula 1 no longer occur. Actually. Until the Bahrain GP. But Romain Grosjean's terrible crash shows that all efforts, including making the drivers' racing overalls more and more fireproof, are not in vain.
Romain Grosjean survived a terrible fire accident at the Bahrain GP.
© FIA / F1
The racing suits are made from a fireproof material called Nomex. In them, the racing drivers can survive temperatures of up to 840 degrees for 35 seconds. It took Grosjean 27 seconds to free himself from the glowing hell. Not only overalls, but also shoes, underwear, gloves and face masks are now made from the special synthetic fiber.
This not only protects drivers from the fire itself, but also from aggressive gases and acids. This is not unimportant, especially with the modern Formula 1 racers. Thanks to the hybrid elements, batteries with toxic materials are also on board. A racing suit costs 1200 euros, weighs 1.9 kilograms and has to withstand a fire of 820 degrees for ten seconds beforehand. That also saved Grosjean, although the Frenchman lost a shoe in his crash.
Grosjean survived mostly because of Halo
But it's not just the racing suits that are safer. Today's cars are also made of carbon fiber and no longer made of easily inflammable magnesium alloys. The fact that Grosjean was not beheaded when it hit the guardrail is thanks to the HALO cockpit protection, which was introduced in 2018 and initially received a lot of criticism. The titanium bar, which is being built in Büren near Paderborn, has to withstand forces of twelve tons from above, 4.7 tons from the front and 9.5 tons from the side. The roll bar on the airbox is now designed for a load of 27 tons.
The safety cell, the so-called monocoque, consists of a Kevlar-carbon composite and is loaded with 20 tons from the front and 25 tons from the side during the crash test. "It's our bulletproof vest," said former world champion Nico Rosberg once. The wheels are also attached to the monocoque with three Kevlar straps.
By the way: The Halo cockpit bar was also introduced because of Jules Bianchi's accident in Suzuka in 2014. Today his mother wrote to a French journalist: "You introduced Halo after my son died, and today he saved Romain's life. That makes me happy."
accident fire Formula Grosjean Hell reports
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You're Just 5 Steps Away from Turning Even a Tiny Audience into a Mass of Buyers!
This is an in-depth video training series. Designed to show you everything you need to know to build up an audience from scratch – or tack onto the audience you've already built for bigger earnings.
There's no guessing here. I'm going to guide you through, step-by-step. So by the end, you'll be set-up and raring to go.
In fact, I'm so confident you're going to enjoy this course (and LOVE the results!), I'm going to tell you exactly what's inside.
This is the research phase to make sure you're targeted profitable niches, and avoiding the money wasters. You'll build a strong foundation, while sealing all the cracks for ongoing success. Giving you peace of mind that your business will never crumble.
The secret method for getting extremely cheap clicks to stretch your advertising budget, while getting the biggest ROI. Separated in 3 core components, this guarantees your ads will be extremely cheap and highly effective.
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You'll get instant access to my personal materials to make the research phase quick and painless.
Selling your product is a breeze… when you have the right offer page. Don't sweat, I'm going to break it down for you. Making the entire process dead simple. By the end, you can be confident your offer page is flawless and ready to draw in your buyers.
How to carefully craft an irresistible hook that will leave your buyers clawing at each other to get inside.
Constructing a product description that will easily turn even the most hesitant visitors into buyers.
Securing the sale and giving your buy button a work out. Warning: this section is crucial and must be done correctly, otherwise you risk losing the sale.
How to shoot a concise demo video that will dramatically cut down your refund rate and workload. Confused buyers will make your life hell. This simple formula will create dedicated buyers that will stick by you for the long haul.
This section is all about keeping your costs down. It's easy to run up an expensive ad bill with little to show for it. Here I will break down how to create highly effective ads for a minimal investment.
The 5 components every high converting ad have must have. With these mastered, your ads will easily attract a ton of clicks with hungry buyers running the mouse.
The secret to choosing a winning image for you ad. And how to avoid a bad picture that will repel your audience.
High converting ad copy that will maximize your clicks. With a well-crafted headline, you'll easily grab the attention of your buyers.
Putting all the pieces together to create a successful ad campaign.
By this section, you'll be able to ramp up into high gear. If you've ever wondering how the million dollar guys are so successful, this is it. Together, we'll make sure your ads are hitting the right people.
The most highly effective ad type available to you, and the perfect conditions to exploit its power.
How to get influential celebrities in your niche working for you. Launching your business to a new level of fame, and creating a recognizable brand your buyers will instantly love.
Showcasing your product, service, software or startup in front of your best audience.
The 5 simple questions that will have you making ad bids like a pro.
Measuring your success is key to ensuring your ads are at optimal performance. This final section will walk you through testing, tweaking and editing to reach your full earning potential. This separates your average hobbyist from a real Facebook ad pro.
Inside look at a private case study that showcases how to split test each ad, from start to finish. This will allow you to make intelligent tweaks for maximum efficiency, without ever taking a shot in the dark that could cost you.
How long to run your tests to ensure you've got adequate data to separate the winners from the losers.
The small tweaks that can transform into huge gains.
Fixing the most common problems that 90% of marketers make. If you're ads aren't gaining traction, these simple techniques will turn your campaign around.
I've broken everything down to make it super simple, and highly effective. So that list your about to breathe some life into will be much, much more valuable to you.
Not only will you see how to create irresistible offer places, this is your opportunity to massively expand your subscribers.


Uber, Air Bnb have transformed their respective industries by bringing in new values and mindset. They have promoted values or concepts related to living in community, sharing, "win win" solutions and this has worked wonderfully well in an era where Millennials are now able to dictate the market.
Creating a "win win" solution and sharing what you have with others are part of the Abundance mindset. People adopting this mindset are more open to working in teams, supporting each other and having a longer term vision. They are willing to try out new concepts and create a whole new dimension of experiences. Someone with an abundance mindset considers any challenge as an opportunity worth taking and any failure as valuable lessons for the future.
Millennials have similar values and mindset. They were born in the globalisation era and have lived in places where it is "normal" to listen to a number of different languages being spoken. They value their freedom to go and do as they please without having to worry about "what others will say or think". For them, their identity is not attached to owning branded products or being seen as living a certain lifestyle. Their identity is more related to what they believe in: fairness, tolerance, flexibility. They would be willing to make a purchase if that purchase supports the cause they believe in.
Making a "quick" profit or buying into a "glamorous" lifestyle is not what they would be supporting. This is similar to having an abundance mindset. Being you and not wanting to compare yourself with others, being appreciative of others and valuing relationships are amongst the various traits of someone having an abundance mindset.
It is difficult to fake an abundance mindset when you don't believe in it. Your actions will not reflect your speech and thoughts. For businesses to tap into this growing generation of millennials, they would probably need to do more than understanding the psychology behind it. They would need to embrace it fully!!! With social media being their main means of communication, a number of Millennials are all about being in the open and sharing their views about everything to everyone. So faking it would only hurt the long term sustainability of your business.
How do you know whether you have an abundance mindset and how do you know whether your business is geared to tap into this growing generation of potential clients, employees and business associates? Here are two tests that help find out for yourself. Abundance Mindset and Are You A Millenial?


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Welcome to Bridgeport, Chicago's oldest and most storied neighborhood, and home to Fabulous Freddies Italian Eatery.
Freddies is Fred and Denise Bertucci's lifelong dream come true. The stars aligned over Bridgeport: Fred fell in love with Denise, and the two perfected their recipes while helping to manage Denise's family's restaurant, and – boom – Freddies was born. And though Bridgeport has changed, Freddies remains constant: It's a family-owned spot that serves awesome fast food made with love from scratch every single day. A business that puts quality over everything (except family). A place where you can get off-menu requests without any hassle. A place where the pricing is always fair and the portions are humongous. A place that changes with the times, but somehow never seems to change.


ONE Firm. ONE Vision. ONE Client at a time.
Let our team of experienced estate planning lawyers develop an asset protection strategy that's customized to your needs. Here at Dvorak Law Group, we are dedicated to providing you and your family with the personal attention that you deserve. Call our Omaha office today at (402) 934-4770, or our Hastings office at (402) 463-3125 for more information on how we can aid you in your estate planning process.
We understand that losing a loved one or making your own arrangements is never easy, and estate planning can be complicated. At Dvorak Law Group we strive to make this difficult and complex time as easy as possible. Our veteran team of estate planning attorneys will help you through the process with a personal touch and a focus on putting you in a position to make educated decisions. Contact us today to discuss how together we can create a plan that will benefit both you and your loved ones.
In the February 3 edition of the Omaha World-Herald, Dvorak Law Group, LLC, ran several announcements. They were located within..
Dvorak Law Group, LLC is pleased to announce that Jeffrey J. Blumel will serve as Managing Partner of the firm,..
Dvorak Law Group, LLC, hosted their annual firm holiday party last week. Employees participated in team building activities, donated items..
OUR ESTATE PLANNING LAWYERS ARE LOOKING OUT FOR YOU.


While waiting to pick up my kids, there are often opportunities to have a quick chat with other mums. I have been having regular chats with one of the mums, all very casual and one day I just invited her along to church and she was open to it. Her children enjoyed KIDS church and she was happy to come along, although religion has always been quite a foreign concept to her.
After several months, she started to attend Alpha and gave her life to Christ, having experienced God's peace and goodness. It's amazing how God uses us just where we are and in the everyday moments.


text:
namespace mojo {

// The test for |MOJO_STATIC_CONST_MEMBER_DEFINITION| is really a compile/link
// test. To test it fully would really require a header file and multiple .cc
// files, but we'll just cursorily verify it.
//
// This is defined outside of an anonymous namespace because
// MOJO_STATIC_CONST_MEMBER_DEFINITION may not be used on internal symbols.
struct StructWithStaticConstMember {
  static const int kStaticConstMember = 123;
};
MOJO_STATIC_CONST_MEMBER_DEFINITION
const int StructWithStaticConstMember::kStaticConstMember;

namespace {

// Note: MSVS is very strict (and arguably buggy) about warnings for classes
// defined in a local scope, so define these globally.
struct TestOverrideBaseClass {
  virtual ~TestOverrideBaseClass() {}
  virtual void ToBeOverridden() {}
  virtual void AlsoToBeOverridden() = 0;
};

struct TestOverrideSubclass : public TestOverrideBaseClass {
  ~TestOverrideSubclass() override {}
  void ToBeOverridden() override {}
  void AlsoToBeOverridden() override {}
};

TEST(MacrosCppTest, Override) {
  TestOverrideSubclass x;
  x.ToBeOverridden();
  x.AlsoToBeOverridden();
}

// Note: MSVS is very strict (and arguably buggy) about warnings for classes
// defined in a local scope, so define these globally.
class TestDisallowCopyAndAssignClass {
 public:
  TestDisallowCopyAndAssignClass() {}
  explicit TestDisallowCopyAndAssignClass(int) {}
  void NoOp() {}

 private:
  MOJO_DISALLOW_COPY_AND_ASSIGN(TestDisallowCopyAndAssignClass);
};

TEST(MacrosCppTest, DisallowCopyAndAssign) {
  TestDisallowCopyAndAssignClass x;
  x.NoOp();
  TestDisallowCopyAndAssignClass y(789);
  y.NoOp();
}

// Test that |MOJO_ARRAYSIZE()| works in a |static_assert()|.
const int kGlobalArray[5] = {1, 2, 3, 4, 5};
static_assert(MOJO_ARRAYSIZE(kGlobalArray) == 5u,
              "MOJO_ARRAY_SIZE() failed in static_assert()");

TEST(MacrosCppTest, ArraySize) {
  double local_array[4] = {6.7, 7.8, 8.9, 9.0};
  // MSVS considers this local variable unused since MOJO_ARRAYSIZE only takes
  // the size of the type of the local and not the values itself.
  MOJO_ALLOW_UNUSED_LOCAL(local_array);
  EXPECT_EQ(4u, MOJO_ARRAYSIZE(local_array));
}

// Note: MSVS is very strict (and arguably buggy) about warnings for classes
// defined in a local scope, so define these globally.
class MoveOnlyInt {
  MOJO_MOVE_ONLY_TYPE(MoveOnlyInt)

 public:
  MoveOnlyInt() : is_set_(false), value_() {}
  explicit MoveOnlyInt(int value) : is_set_(true), value_(value) {}
  ~MoveOnlyInt() {}

  // Move-only constructor and operator=.
  MoveOnlyInt(MoveOnlyInt&& other) { *this = std::move(other); }
  MoveOnlyInt& operator=(MoveOnlyInt&& other) {
    if (&other != this) {
      is_set_ = other.is_set_;
      value_ = other.value_;
      other.is_set_ = false;
    }
    return *this;
  }

  int value() const {
    assert(is_set());
    return value_;
  }
  bool is_set() const { return is_set_; }

 private:
  bool is_set_;
  int value_;
};

TEST(MacrosCppTest, MoveOnlyType) {
  MoveOnlyInt x(123);
  EXPECT_TRUE(x.is_set());
  EXPECT_EQ(123, x.value());
  MoveOnlyInt y;
  EXPECT_FALSE(y.is_set());
  y = std::move(x);
  EXPECT_FALSE(x.is_set());
  EXPECT_TRUE(y.is_set());
  EXPECT_EQ(123, y.value());
  MoveOnlyInt z(std::move(y));
  EXPECT_FALSE(y.is_set());
  EXPECT_TRUE(z.is_set());
  EXPECT_EQ(123, z.value());
}

// Use it, to make sure things get linked in and to avoid any warnings about
// unused things.
TEST(MacrosCppTest, StaticConstMemberDefinition) {
  EXPECT_EQ(123, StructWithStaticConstMember::kStaticConstMember);
}

// The test for |ignore_result()| is also just a compilation test. (Note that
// |MOJO_WARN_UNUSED_RESULT| can only be used in the prototype.
int ReturnsIntYouMustUse() MOJO_WARN_UNUSED_RESULT;

int ReturnsIntYouMustUse() {
  return 123;
}

TEST(MacrosCppTest, IgnoreResult) {
  ignore_result(ReturnsIntYouMustUse());
}

}  // namespace
}  // namespace mojo

redpajama_set_name: RedPajamaGithub


Should I buy a DI?
The right stuff for bass traps?
TLA M3 Tubetracker DO-1 digital option card?
is my digi pre f#!!*d.
What Studio Desk Is This?????
Front end for a Digi002??
PTHD 192 interface- analog insterts-Latency question..
Is this a good deal for an Ampeg B-25b?
It's here! Digidesign 003 pictures.
Phoenix Audio - N16 Safe to buy?
Faders or No Faders with Summing Mixer?
Hi guys. Have been looking through emperical labs web site and can find nothing on the brit mod. What is the brit mod?


The Chamber is a volunteer organization of business and professional men and women who have joined together for the purpose of promotion the civic and economic progress of our community.
The Chamber's Military Affairs Committee is the oldest military affairs committee in the Marine Corps hosts' communities. The Chamber's reach also extends past the county line to Raleigh and even Washington, D.C with Government Affairs Committee.
The Chamber has an over 70 year tradition, acting as a voice for businesses in Jacksonville and Onslow County. The Jacksonville•Onslow Chamber of Commerce is vigilant in Connecting Business, Military, and Community.
Our sincere thanks to UNCW, The Jacksonville-Onslow Chamber of Commerce and all other participants for making this another great Whole Vet event! Please check our Events Page often for updates and upcoming events.


I am a benthic ecologist focussing on the deep sea and Arctic ecosystems, specifically studying the impacts of biotic, abiotic and anthropogenic inputs on the faunal community. I am increasingly focussing on the distribution and abundance of microplastics in the world's oceans.
I am also the Head of SAMS' Graduate School.
The deep sea is by far the largest ecosystem on the planet. It harbours many fascinating habitats including underwater mountains through to the nearby continental margins. My deep-sea research interests are in the diversity, composition and structure of the deep water fauna living on or in the sediments and how these relate to the different environmental variables that interact and influence the fauna, ranging from, changes in temperature as a result of internal tides, to habitat heterogeneity and impacts from a changing climate. I am particularly interested in the fauna that live on seamounts and banks as well as the soft sediment found on the continental margins in all the major oceans including the NE Atlantic and polar seas.
In addition my research focus is looking at plastics, specifically microplastics, found in the marine environment. Microplastics, particles < 5 mm in size, are of particular biological concern as they can be ingested by a wide diversity of organisms, which have been shown to suffer negative impacts as a consequence. The long term fate of marine microplastics is not well known; however it is hypothesised that the deep sea may be the final repository for this pollutant. Assessing the input sources, transport routes and 'lifecycle' of marine microplastics are fundamental questions to understanding the impacts of plastic pollution and ensure adequate mitigation measures are in place at both a regional and global level.
Watson C, Chivers AJ, Narayanaswamy BE, Lamont P & Turnewitsch R (2014) Chrysopetalidae (Annelida: Phyllodocida) from Senghor Seamount, NE Atlantic: taxa with deep-sea affinities & morphological adaptions. Memoirs of the Museum of Victoria: Proceedings of the International Polychaete Conference 71: 311-325.
Thurber AR, Sweetman AK, Narayanaswamy BE, Jones DOB, Ingels J & Hansman RL (2014). Ecosystem function and services provided by the deep sea. Biogeosciences 11, 3941-3963.
Narayanaswamy BE, Coll M, Danovaro R, Davidson K, Ojaveer H & Renaud PE (2013). Synthesis of knowledge on marine biodiversity in European Seas: from Census to sustainable management. PLoS ONE 8(3): e58909.
Jeffreys RM, Burke C, Jamieson AJJ, Narayanaswamy BE, Ruhl HA, Smith Jr KL, Witte U (2013) Feeding preferences of abyssal macrofauna inferred from in-situ pulse chase experiments. PLoS ONE 8:11 e80510.
Hughes DJ & Narayanaswamy BE (2013). Impacts of climate change on deep-sea habitats. Marine Climate Change Impacts Partnership: Science Review. pp 204-210.
Narayanaswamy BE, Hughes DJ, Howell KL, Davies J & Jacobs C. (2013) First observations of megafaunal communities inhabiting George Bligh Bank, Northeast Atlantic. Deep Sea Research II. 92:79-86.
Serpetti N, Gontikaki E, Narayanaswamy BE & Witte U (2013) Macrofauna community inside and outside of the Darwin Mounds SAC, NE Atlantic. Biogeosciences, 10, 3705– 3714.
Chivers AJ, Narayanaswamy BE, Lamont PA, Dale A & Turnewitsch R (2013) Changes in polychaete standing stock and diversity on the northern side of Senghor seamount (NE Atlantic). Biogeosciences, 10, 3535– 3546.
Morato T, Kvile K Ø, Taranto GH, Tempera F, Narayanaswamy BE, Hebbeln D, Menezes GM, Wienberg C, Santos RS & Pitcher TJ (2013) Seamount physiography and biology in the north-east Atlantic and Mediterranean Sea. Biogeosciences, 10, 3039–3054.
Gontikaki E, Polymenakou PN, Thornton B, Narayanaswamy BE, Black K, Tselepides A & Witte U. (2012) Microbial response to organic matter enrichment in the oligotrophic Levantine Basin (Eastern Mediterranean). Geomicrobiology Journal. 29 (7) 648-655.
Fehling J, Davidson K, Bolch CJS, Brand T & Narayanaswamy BE (2012) Autumnal phytoplankton distribution in North West European shelf sea waters with special emphasis on the diatom. PLoS ONE 7 (3): e34098.
Gontikaki E, Mayor DJ, Narayanaswamy BE & Witte U (itemIDitemID2331E2011) Feeding strategies of deep-sea sub-Arctic macrofauna of the Faroe-Shetland Channel: combining natural stable isotopes and enrichment techniquesuserIDuserID56E. Deep-sea Res I. 58:160-172.
Narayanaswamy BE & Bett BJ. (2011) Macrobenthic biomass relations in the Faroe-Shetland Channel: An Arctic-Atlantic boundary environment. PLoS ONE 6(4): e18602.
Wei C-L, Rowe GT, Escobar-Briones E, Boetius A, Soltwedel T, Caley MJ, Soliman Y, Huettmann F, Qu F, Yu Z, Pitcher CR, Haedrich RL, Wicksten MK, Rex MA, Baguley JG, Sharma J, Danovaro R, MacDonald IR, Nunnally CC, Deming JW, Montagna P, Lévesque M, Weslawski JM, Wlodarska-Kowalczuk M, Ingole BS, Bett BJ, Billet D, Yool A, Bluhm BA, Iken K & Narayanaswamy BE (2010) Global Patterns and predictions of seafloor biomass using Random Forests. PLoS ONE. 5(12) e:15323.
Narayanaswamy BE, Renaud P, Duineveld G, Berge J, Lavaleye MSS, Reiss H & Brattegard T (itemIDitemID2328E2010). Biodiversity trends along the western European MarginuserIDuserID56E. PLoS ONE. 5 (12):e14295.
Ramirez-Llodra E, Brandt A, Danovaro R, De Mol B, Escobar E, German C, Levin L, Martinez-Arbizu P, Menot L, Buhl-Mortensen P, Narayanaswamy BE, Smith CR, Tittensor D, Tyler P, Vanreusel A & Vecchione M (itemIDitemID2316E2010) Deep, diverse and definitely different: unique attributes of the world's largest ecosystemuserIDuserID56E. Biogeosciences. 7: 2851-2899.
Narayanaswamy BE, BJ Bett & Hughes DJ (itemIDitemID2243E2010) Deep-water macrofaunal diversity in the Faroe-Shetland region (NE Atlantic): a margin subject to an unusual thermal regimeuserIDuserID56E. Marine Ecology. 31: 237-246.
Howell K, Davies JS & Narayanaswamy BE (itemIDitemID2242E2010) Identifying deep-sea megafaunal epibenthic assemblages for use in habitat mapping and marine protected area network designuserIDuserID56E. JMBA UK. 90: 33-68.
Narayanaswamy BE & Blake JA (itemIDitemID984E2005). A new species of Orbiniella (Polycahaeta: Orbiniidae) from deep basins of AntarcticauserIDuserID56E. JMBA UK. 85(4): 843-846.
Narayanaswamy BE Bett BJ & Gage JD (itemIDitemID983E2005). Ecology of bathyal polychaete fauna at an Arctic-Atlantic boundary (Faroe-Shetland Channel, North-east Atlantic)userIDuserID56E. Marine Biology Research. 1: 20-32.
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Narayanaswamy BE, Nickell TD & Gage JD (itemIDitemID370E2003) Appropriate levels of taxonomic discrimination in deep-sea studies: species vs familyuserIDuserID56E. Mar Ecol Prog Ser. 257: 59-68.
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Ingels J, Clark M, Vecchione M, Perez JAA, Levin L, Priede IG, Sutton T, Rowden AA, Smith CR, Yasuhara M, Sweetman AK, Soltwedel T, Santos R, Narayanaswamy BE, Ruhl HA, Fujikura K, Amaral Zettler L, Jones DOB, Gates AR, Snelgrove P, Bernal P & van Gaever S (2016) Open Ocean Deep Sea. IN: Oceans and Law of the Sea – United Nations. Ch 36F.
Baker E, Gaill F, Karageirgis AP, Lamarche G, Narayanaswamy BE, Parr J, Raharimananirina C, Santos R, Sharma R & Tuhumwire J (2016). Offshore Mining Industries. IN: Oceans and Law of the Sea – United Nations. Ch 23.
I have 15+ years of experience working on the biology of deep-sea ecosystems. Some of this work has been undertaken through the Strategic Environmental Surveys of the deep waters around the UK.


Police officers came across a group of more than 20 Asian men fighting on Princess Street at around 10pm on Wednesday, April 10.
Two men have been charged following a large scale brawl in Great Harwood.
Officers said weapons were used including a cricket bat which has now been recovered.
A man was taken to hospital with minor injuries and no other injuries were reported.
A Lancashire Police spokesperson said they do not know what caused the brawl and are investigating.
They are also seeking to speak to a number of men about the fight.
A 43-year-old and a 23-year-old have been charged with a section 4 public order offence by using words and behaviour to cause fear of unlawful violence.
Both men have been bailed to appear before Blackburn Magistrates Court on Friday, April 26.
Councillor Ian Robinson said the problem has been going on for a 'long time' and is looking to organise a meeting with residents and the police about the issue.
Police have increased patrols in the area and anyone with information is being urged to call Eastern CID on 101.