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

The 5.8 Gyr-old \citep{mam08}
main-sequence G8.5V star $\tau$ Ceti is the second closest \cite[3.65~pc,][]{vanL07} Solar-type star
reported to harbor both a tentative planetary system and a debris disk
\cite[after $\epsilon$ Eridani, e.g.][]{gre98,hat00}.  The $\tau$ Ceti debris disk was
first identified as an infrared excess by IRAS \citep{aum85} and
confirmed by ISO \citep{hab01}.  \cite{gre04} marginally resolved 850 $\mu$m
emission from the system with the James Clerk Maxwell Telescope (JCMT)/SCUBA,
revealing a massive (1.2 $M_\oplus$) disk extending to 55 AU from the star.  Recent \emph{Herschel}
observations at 70, 160, and 250~$\mu$m resolve the disk well and are best fit
by a broad dust belt with an inner edge between $1-10$ AU and an outer edge at
$\sim55$~AU \citep{law14}.  Due to its proximity and similarity to our Sun in age and spectral type, $\tau$ Ceti has been the
object of numerous searches for planets using the radial velocity technique
\cite[e.g.][]{pepe11}, most of which have proved unsuccessful.
Using extensive modeling and Bayesian analysis of radial velocity data from the High Accuracy Radial Velocity Planet Searcher (HARPS) spectrograph \citep{may03,pepe11}, the Anglo-Australian Planet Search (AAPS) on the Anglo Australian Telescope (AAT),
and the High Resolution Echelle Spectrograph (HIRES) on the Keck telescope \citep{vogt94}, \cite{tuo13} report evidence for a tightly-packed five planet system.
This purported planetary system consists of five super-Earths
with masses of $4.0-13.2$~$M_\oplus$ (for orbits co-planar with the disk), semi-major axes
ranging over $0.105-1.35$ AU, and small eccentricities, $e\sim0-0.2$.
The veracity of these planet candidates, however, remains controversial.  \cite{tuo13} acknowledge
that the detected signals could also result from a combination of instrumental bias
and stellar activity, although no further evidence is given to support these alternative
interpretations.  Also of note is the sub-Solar metallicity of $\tau$ Ceti, [Fe/H] $= -0.55\pm0.05$ dex \citep{pav12}, which makes it an interesting target for exoplanet searches due to the observed higher frequency of low-mass planets around low-metallicity stars \citep{jen13}.

We present interferometric observations of the $\tau$ Ceti system at
1.3~mm using the Atacama Large Millimeter/submillimeter Array (ALMA).
Millimeter imaging of this debris disk opens a unique window on the location
and morphology of the underlying population of dust-producing planetesimals
orbiting the star.  While these large, kilometer-sized bodies cannot be
detected directly, millimeter observations probe emission from the large dust
grains produced through collisions that are not rapidly redistributed by stellar radiation and winds \citep{wya06}.
These new ALMA observations provide limits on the disk location and width,
which bear on the proposed planetary system within the disk.
In Section~\ref{sec:obs}, we present the ALMA observations of the $\tau$ Ceti
system.  In Section~\ref{sec:results}, we describe the analysis technique
and disk model results.  In Section~\ref{sec:disc}, we discuss the significance of the best-fit model parameters for
the dust belt inner edge, width, proposed planetary
system, and the origin of a bright, unresolved central emission source.

\section{Observations}
\label{sec:obs}

The $\tau$ Ceti system was observed using Band 6 (1.3~mm) in December 2014 with the ALMA 12-m array.  We obtained one scheduling block (SB) in good weather (PWV = 1.76~mm) with 34 antennas, with the longest baselines sampling to $1\arcsec$ ($4$ AU) resolution.
These observations were complemented by two SBs taken with the Atacama Compact
Array (ACA) in July 2014 to provide shorter baselines and sensitivity to
emission at larger scales.  For these ACA SBs, 11 operational antennas were
available.  The observation dates, baseline lengths, and total time on-source are summarized in Table~\ref{tab:obs}.
For maximum continuum sensitivity, the correlator was configured to process two
polarizations in four 2 GHz-wide basebands
centered at 226, 228, 242, and 244~GHz, each with 256 spectral channels.
For the July SBs, the phase center was
$\alpha = 01^\text{h}44^\text{m}02.348$,
$\delta = -15\degr56\arcmin02\farcs509$ (J2000, ICRS reference frame).  The phase center for the December SB
was $\alpha = 01^\text{h}44^\text{m}02.299$,
$\delta = -15\degr56\arcmin02\farcs154$ (J2000, ICRS reference frame).  Both phase centers were chosen to be the
position of $\tau$ Ceti at the time of the observations given its proper motion of ($-1721.05$, $854.16$)
mas yr$^{-1}$ \citep{vanL07}.
The field of view is $\sim26\arcsec$, given by the FWHM size of the primary beam the ALMA 12-m antennas at the mean frequency of 234 GHz.

The data from all three SBs were calibrated separately using the \texttt{CASA}
software package (version 4.2.2).  We corrected for time-dependent complex gain variations using
interleaved observations of the calibrator J0132-1654.  Observations of J0137-2430 were used to determine the spectral response
of the system. The absolute flux calibration scale was derived from observations of Neptune, and a mean calibration
was applied to all four basebands, with a systematic uncertainty of $\sim10\%$ \cite[see][for a complete discussion of flux density models of Solar System bodies]{but12}.

To generate a first image at the mean frequency, 234~GHz (1.3~mm), we Fourier inverted the calibrated visibilities with natural weighting and a multi-frequency synthesis with the \texttt{CLEAN} algorithm.  To improve surface brightness sensitivity, we included a modest taper using the \texttt{uvtaper} parameter in \texttt{CLEAN}, which controls the radial weighting of visibilities in the $(u,v)$-plane through the multiplication of the visibilities by the Fourier transform of a circular Gaussian (on-sky FWHM $= 6\arcsec$).  With the added taper, however, it became difficult to resolve the outer disk and the central stellar emission.  For clarity, we chose to image the disk and the star separately.  We isolate the disk emission by subtracting a point source model from these data using the CASA task \texttt{uvsub} to account for the stellar emission.  To isolate the stellar component, we image with \texttt{CLEAN} and no taper, only including baselines longer than 40 k$\lambda$, where we expect the star to dominate the emission (see Section~\ref{sec:results}). We choose to account for the primary beam in our modeling (see Section~\ref{subsec:modeling}) and thus do not apply a primary beam correction to any of these images.

\section{Results and Analysis}
\label{sec:results}

\subsection{Continuum Emission}
\label{subsec:continuum}

Figure~\ref{fig:images} shows an ALMA 1.3 mm image of the $\tau$ Ceti disk made
with the central star subtracted (middle panel) along with an image including
only baselines longer than 40 k$\lambda$ showing emission from the star and
not the disk (right panel).  The \emph{Herschel/PACS} 70 $\mu$m star-subtracted
image (left panel) is shown for reference \citep{law14}.
The natural weight rms noise is 30 $\mu$Jy and 180 $\mu$Jy for the 12-m and ACA observations, respectively.
For the image showing only the stellar emission, the natural weight rms is
higher, 35 $\mu$Jy, since we exclude some baselines.
The belt is not detected in the ACA observations given the low signal-to-noise ratio, and
we only consider the 12-m data for imaging and modeling (see Section~\ref{subsec:modeling}).
For the 1.3~mm image of the star, the synthesized beam with natural weighting
is $1\farcs9\times1\farcs0$ ($7\times4$~AU), and position angle $= -87\degr$.
To improve surface brightness sensitivity, the image of the disk makes use of
a modest taper and has a synthesized beam size of $6\farcs5\times6\farcs1$
($24\times22$~AU), and position angle $= 55\degr$.

These 1.3~mm images reveal (1) patchy emission ($\sim6\sigma$) from a nearly face-on (low inclination) dust disk,
and (2) a bright ($23\sigma$), unresolved central peak coincident with the expected stellar position.  The disk is located $\sim12\arcsec$ ($\sim44$~AU) from the star with a position angle of $\sim90\degr$ (E of N).  \cite{rei88} quantify the position uncertainty, $\sigma$ of a point source given the signal-to-noise ratio, $S/N$, and the synthesized beam size, $\theta$: $\sigma \sim 0.5\theta/(S/N)\approx 0\farcs14$, for our observations.  The position of the observed central source is coincident with the expected stellar position within this uncertainty.

\begin{figure}[ht]
\begin{minipage}[h]{0.37\textwidth}
  \begin{center}
       \includegraphics[scale=0.5]{fig1a}
  \end{center}
 \end{minipage}
 \begin{minipage}[h]{0.3\textwidth}
  \begin{center}
       \includegraphics[scale=0.5]{fig1b}
  \end{center}
 \end{minipage}
  \begin{minipage}[h]{0.3\textwidth}
  \begin{center}
       \includegraphics[scale=0.5]{fig1c}
    \end{center}
  \end{minipage}
\caption{\small \emph{(left)} \emph{Herschel/PACS} map of the 70~$\mu$m emission from the $\tau$ Ceti debris disk with the stellar contribution subtracted \cite[see][]{law14}.  The \emph{Herschel} $5\farcs6$ beam size is shown by the ellipse in the lower left corner.
\emph{(center)} The $\tau$ Ceti debris disk imaged by ALMA at 1.3~mm with contours in steps of $2\sigma$, where $\sigma$ is the rms noise level in the image $\sim30$~$\mu$Jy.  To isolate the disk emission, a point source model has been subtracted to account for the central stellar emission.  Using natural weighting along with a $6\arcsec$ Gaussian taper, the resulting FWHM synthesized beam size is $6\farcs5\times6\farcs1$.
\emph{(right)} ALMA image of the 1.3~mm continuum emission for baselines longer than 40~k$\lambda$ showing only the central point source with contours in steps of $5\sigma$.  Imaging with natural weighting and no taper yields a FWHM synthesized beam size of $1\farcs9\times1\farcs0$.
The position of the stellar photosphere is indicated in the left two panels by the blue star symbol.  The primary beam of the ALMA antennas at 1.3~mm (FWHM $\sim26\arcsec$) is shown by the dashed blue circle in the right two panels.
}
\label{fig:images}
\end{figure}

\subsection{Emission Modeling Procedure}
\label{subsec:modeling}

We make use of the modeling scheme described in \cite{mac13,mac15b}.  In this approach, we construct parametric models of the 1.3~mm disk emission and then compute corresponding model visibilities using a python implementation\footnote{The code used to perform this part of the analysis is open source and freely available at \texttt{https:$//$github.com$/$AstroChem$/$vis\_sample}.} of the Miriad \texttt{uvmodel} task (Loomis et al. in prep).  To determine the best-fit parameter values and their uncertainties, we employ the \texttt{emcee} Markov Chain Monte Carlo (MCMC) package \citep{for13}.  This affine-invariant ensemble sampler for MCMC, enables us to accurately sample the posterior probability functions of all model parameters with minimal fine-tuning.  Due to the much higher rms noise of the ACA data, we choose to only fit models to the visibilities from the full 12-m ALMA array.

We model the millimeter emission of the $\tau$ Ceti debris disk as an axisymmetric, geometrically thin belt with an inner radius, $R_\text{in}$, an outer radius, $R_\text{out}$, and a radial surface brightness distribution described by a simple power law, $I_\nu \propto r^{\gamma-0.5}$.
Here, $\gamma$ describes the power law in radial surface density,
$\Sigma \propto r^\gamma$, and temperature is assumed to follow a power law,
$T\propto r^{-0.5}$, approximating radiative equilibrium for blackbody grains.  To first order, the dust temperature also depends on the grain opacity, $T\propto r^{-2/(4+\beta)}$, where $\beta$ is the power law index of the grain opacity as a function of frequency, $\kappa_\nu\propto\nu^\beta$.  \cite{gas12} measure $\beta = 0.58$, from observations of debris disks, which implies a temperature power law index of $\sim-0.44$.  Thus, the expected change in the temperature profile due to $\beta$ is much smaller than the uncertainty in our resulting model fits and we choose to ignore this effect.  Furthermore, the surface density and temperature profiles are degenerate, so we assume a blackbody profile and fit only for $\gamma$.

We constrain the outer disk radius using previous JCMT/SCUBA observations \citep{gre04}, since the parent body disk may have a different size relative to the smaller grains imaged with \emph{Herschel}.  While \cite{gre04} suggested that the disk was highly inclined, the \emph{Herschel} image (Figure~\ref{fig:images}, left panel) indicates that it is closer to face-on.  The SCUBA image is therefore marginally resolved at best, so we take their derived disk radius of 55~AU as an upper limit on $R_\text{out}$ and allow the inner radius, $R_\text{in}$, to vary.  We fit for the surface density radial power law index, $\gamma$, within a range of $-4$ to $4$.  The unresolved central peak seen in images is modeled by a central point source with flux, $F_\text{cen}$.  We do not fit for any relative offsets of the belt center, point source position, and phase center.
Models of the \emph{Herschel} images derive an inclination of $i = 35\degr\pm10\degr$ and position angle, $PA = 105\degr\pm10\degr$ \citep{law14}, and we assume that the millimeter belt emission is described by the same geometry.  For all parameters, we assume uniform priors and require that the model be physically plausible: $F_\text{cen} \geq 0$, and $0 \leq R_\text{in} < R_\text{out} \leq 55$~AU.

A total flux density, $F_\text{belt} = \int I_\nu d\Omega$, provides the normalization for the belt emission.  Using SCUBA on the JCMT, \cite{gre04} obtain a total flux density at 850 $\mu$m for the disk of $5.8\pm0.6$~mJy, including both the central star and likely contamination from background sources.  Recent SCUBA-2 observations at 850 $\mu$m yield a total flux density of $4.5\pm0.9$~mJy, including a contribution from the star of $\sim1$ mJy (Holland et al., in prep.).  An extrapolation of this measurement using the typical spectral index of 2.58 for debris disks at (sub)millimeter wavelengths \citep{gas12}, yields an expected flux density of the disk at 1.3 mm of $1.2\pm0.2$~mJy.  This more robust single-dish flux measurement allows us to constrain the total flux density of our models with a Gaussian prior, $0.6\text{ mJy}\leq F_\text{belt}\leq1.6\text{ mJy}$, accounting for uncertainty in both the single-dish 850~$\mu$m flux measurement and the extrapolation to 1.3~mm.

The angular scale of the $\tau$ Ceti debris disk is $\sim25\arcsec$ in diameter.  At 1.3~mm, the half power field of view of the 12-m ALMA antennas is comparable, FWHM$\sim26\arcsec$.  Given this, we must account for the effect of the primary beam response on our model parameters.  To do this, we model the ALMA primary beam as a Gaussian normalized to unity at the beam center and multiply each parametric disk model by this Gaussian beam model.  Since we account for the effect of the primary beam in our modeling scheme, we choose not to apply a primary beam correction to the images shown in Figure~\ref{fig:images} (right panels).

\subsection{Results of Model Fits}
\label{subsec:model_fits}

Modeling the ALMA 1.3~mm visibilities yields a final best-fit model with a reduced $\chi^2$ value of 1.1.  Table~\ref{tab:mcmc} lists the best-fit values for each of the 5 free parameters along with their corresponding $1\sigma$ ($68\%$) uncertainties.  The 1D (diagonal panels) and 2D (off-diagonal panels) projections of the posterior probability distributions for all parameters except the total belt flux, $F_\text{belt}$, are shown in Figure~\ref{fig:mcmc}.  A full resolution image of this best-fit model (with a flat surface density profile, $\gamma=0$, and the central star excluded) is shown in the leftmost panel of Figure~\ref{fig:model}.  The same model convolved with the $\sim6\arcsec$ ALMA synthesized beam and imaged like the observations in Figure~\ref{fig:images} is shown in the next two panels both without (left) and with (right) simulated random noise with an rms of 30~$\mu$Jy.  Including the simulated noise results in a patchy image with emission structure similar to the ALMA 1.3~mm image shown in Figure~\ref{fig:images}.  In both the ALMA and model images, the most significant peaks of emission are consistent with the expectation for a slightly inclined disk with PA near $90\degr$.  The rightmost panel of Figure~\ref{fig:model} shows the residuals resulting from subtracting this best-fit model from the observed visibilities, again imaged with the same parameters.  No significant features are evident.

\begin{figure}[ht]
\centerline{\psfig{file=fig2,width=10cm,angle=0}}
\caption[]{\small The 1D (diagonal panels) and 2D (off-diagonal panels) projections of the posterior probability distributions for the best-fit model parameters ($R_\text{in}$, $R_\text{out}$, $F_\text{cen}$, and $\gamma$) resulting from $\sim10^4$ MCMC trials.  For a given parameter, the 1D distribution is determined by marginalizing over all other model parameters.  The best-fit parameter value is indicated by the vertical blue dashed line.  The 2D joint probability distributions show the $1\sigma$ (red) and $2\sigma$ (gray) regions for all parameter pairs, with the best-fit parameter values marked by the blue cross symbol.
}
\label{fig:mcmc}
\end{figure}

The best-fit total belt flux density is $F_\text{belt} = 1.0^{+0.6}_{-0.4}$~mJy, constrained by the Gaussian prior taken from previous single dish flux measurements.  \cite{law14} note that the SCUBA and SCUBA-2 flux densities are higher than expected given an extrapolation from the \emph{Herschel} flux density measurements.  This difference suggests that these earlier observations could be contaminated by the extragalactic background or that the disk could have an additional warm component.  Given the limits in sensitivity of our ALMA data, the total flux density we measure is consistent with both the \emph{Herschel} and SCUBA/SCUBA-2 values and we cannot distinguish between these two scenarios.

Not surprisingly, given the sensitivity limits of the ALMA data, model fitting does not provide a strong constraint on the power law index of the surface density radial profile, $\gamma=-0.3^{+1.9}_{-1.3}$.  With large uncertainty, this result implies a shallow surface density profile.  In addition, we see a clear degeneracy between the surface density gradient, $\gamma$, and the disk outer radius, $R_\text{out}$ \cite[e.g.][]{mun96}.  For very negative values of $\gamma$, the outer regions of the resulting belt model have low surface brightness, making it difficult to constrain the position of the outer edge.  Thus, the contours shown in Figure~\ref{fig:mcmc} for that pair of parameters exhibit a slope, spreading out to span a wide range of possible outer radii for increasingly negative values of $\gamma$.

\begin{figure}[ht]
\centerline{\psfig{file=fig3,width=16cm,angle=0}}
\caption[]{\small  \emph{(left)} A full resolution (pixel scale $\sim0\farcs05\sim0.2$~AU) image of the best-fit model to the 1.3~mm ALMA continuum emission.  For simplicity, we have chosen a flat surface density profile with $\gamma=0$ and excluded the central stellar component.  \emph{(center left)} The same best-fit model convolved with the $\sim6\arcsec$ ALMA synthesized beam and imaged as in Figure~\ref{fig:images}, but with no noise added. \emph{(center right)}  The convolved best-fit model (same as shown in center left) with added simulated random noise at the same level as the ALMA 1.3~mm image, rms $\sim30$~$\mu$Jy. \emph{(right)} The residuals of the full best-fit model including the star and imaged with the same parameters as in Figure~\ref{fig:images}.  The ellipse in the lower left corner shows the $6\farcs5\times6\farcs1$ (FWHM) synthesized beam size.
}
\label{fig:model}
\end{figure}

Another helpful way to visualize and compare the ALMA observations and the best-fit model is by deprojecting the real and imaginary visibilities based on the inclination, $i$, and position angles, $PA$, of the disk major axis, as is shown in Figure~\ref{fig:vis} \cite[see][for a detailed description of deprojection]{lay97}.  Essentially, the coordinates for each visibility point are defined by a distance from the origin of the $(u,v)$ plane, $\mathcal{R} = \sqrt{u^2+v^2}$. To change to a deprojected, rotated coordinate system, we define an angle $\phi = \frac{\pi}{2}-PA$, where $PA$ is the position angle of the disk measured east of north.  The new coordinates are defined as $u' = u\text{ cos}\phi+v\text{ sin}\phi$ and $v' = (-u\text{ sin}\phi+v\text{ cos}\phi)\text{ cos}i$, where $i$ is the inclination angle of the disk.  Then, the new deprojected $(u,v)$ distance is $\mathcal{R}_{uv} = \sqrt{u'^2+v'^2}$.  Assuming that the disk is axisymmetric, we average the visibilities azimuthally in annuli of $\mathcal{R}_{uv}$.  For our ALMA $\tau$ Ceti observations, the real part of the deprojected visibilities is reasonably consistent with the prediction for a broad belt of emission, showing a central peak and several oscillations of decreasing amplitude.  The constant offset from zero is the visibility signature of the unresolved central peak we see clearly in the images.  The imaginary visibilities are essentially zero, indicating that there is no asymmetric structure in the disk, which is consistent with the absence of any significant residuals in Figure~\ref{fig:model} (rightmost panel).  Note that we are lacking $(u,v)$ coverage on baselines shorter than $\lesssim20$ k$\lambda$, the region of the visibility curve with the most structure.

\begin{figure}[ht]
\centerline{\psfig{file=fig4,width=10cm,angle=0}}
\caption[]{\small The deprojected real (filled symbols) and imaginary (open symbols) visibilities for the ACA (blue diamonds) and 12-m array (black circles), compared to the best-fit belt model (red solid line).  The single dish SCUBA-2 flux (Holland et al., in prep.) extrapolated from 850 $\mu$m to 1.3 mm is also plotted at $\mathcal{R}_{uv} = 0$ k$\lambda$.
}
\label{fig:vis}
\end{figure}

\section{Discussion}
\label{sec:disc}

We have obtained ALMA 1.3~mm observations of the $\tau$ Ceti system using both the ACA and the full 12-m array with baselines corresponding to scales of $1\arcsec$ ($4$ AU). The resulting image shows emission from an outer dust disk located $\sim12\arcsec$ ($\sim44$ AU) from the star surrounding an unresolved central peak.  We fit parametric models to the millimeter visibilities, which included two components: (1) an outer disk with a radial surface density profile described by a power law with index $\gamma$, and (2) a point source at the stellar position.  In the context of our simple model, this analysis provides tentative constraints on the location of the disk inner edge and the width of the disk.  We now compare the model fits to previous \emph{Herschel} observations and discuss implications for the geometry of the proposed inner planetary system located within the dust belt.

\subsection{Location of the Disk Inner Edge and Belt Width}
\label{subsec:inner_edge}

Our best-fit model yields an inner radius for the disk of $6.2^{+9.8}_{-4.6}$~AU, consistent with the analysis of \emph{Herschel} observations that constrained the inner edge of the disk to be between 1 and 10~AU from the star \citep{law14}.  For comparison, the planetary system proposed by \cite{tuo13} consists of five super-Earths in a tightly-packed configuration with semi-major axes ranging over $0.105-1.35$~AU.  Given the uncertainties on $R_\text{in}$ from our best-fit model, the disk could extend well into this inner planetary system ($R_\text{in} < 1$ AU) or end far beyond the outermost planet ($R_\text{in} > 2$ AU).  None of the proposed planets have large enough orbital radius or mass to cause significant perturbations or clear the disk beyond 3 AU (within the range of $R_\text{in}$ allowed by our models). Lawler et al. (2014) use numerical simulations to show that the system would be stable with an additional Neptune-mass planet on an orbit of $5-10$ AU, the largest mass planet at such separations that cannot be ruled out by the radial velocity data.

\begin{figure}[ht]
\centerline{\psfig{file=fig5,width=14cm,angle=0}}
\caption[]{\small \emph{(left)}~The deprojected real component of the expected complex visibilities for belt models with our best-fit $R_\text{in}=6.2$~AU and $\gamma=-1,0,+1$ (dot-dash green line, solid red line, and dotted purple line, respectively), and a model with $R_\text{in} = 20$~AU and $\gamma=0$ (dashed blue line).  The real visibilities from our ACA observations presented here are shown by the black points and are consistent with all four models.
\emph{(center)}~The real visibilities of simulated ACA 1.3~mm emission for models with $\gamma=0$ and $R_\text{in}=6.2$ and $20$~AU (red and blue points, respectively).  With 10 antennas and 10 hours on source, these models are easily distinguishable.
\emph{(right)}~The real visibilities of simulated ACA 1.3~mm emission for models with $R_\text{in}=6.2$~AU and $\gamma=+1$ and $-1$ (purple and green points, respectively).  Again, these profiles are clearly different in shape, with the zero-crossing null locations shifted by $>10$ k$\lambda$.
}
\label{fig:sim}
\end{figure}

The belt position and width are strongly constrained by the location of the first null in the deprojected real visibilities \cite[see Figure~\ref{fig:vis},][]{mac15b}.  Although we obtained some ACA data, the integration time was short, and the resulting sensitivity (rms $\sim180$~$\mu$Jy) at short baselines ($< 20$~k$\lambda$) was insufficient to discriminate between disk models with inner radii of $1-10$~AU, the parameter space with significant implications for the proposed planetary system.  New observations with shorter baselines are needed to better determine the location of the dust belt, as well as its radial surface density gradient. To demonstrate the contribution that such observations would make to our analysis, we carried out simulations of ALMA ACA observations (rms 60~$\mu$Jy, using 10 antennas in the Cycle 4 setup) at 1.3~mm for a model with our best-fit $R_\text{in} = 6.2$ AU and $\gamma=-1,0,+1$,  and a model with $R_\text{in} = 20$ AU and $\gamma=0$, all consistent with the ALMA observations presented here. Figure~\ref{fig:sim} (left panel) shows the real component of the expected complex visibilities for all four models, along with our current ACA observations.  The center and right panels show the real part of simulated ACA visibilities for all four belt models compared to the expected theoretical visibility curves.  These profiles are clearly different in shape, with the zero-crossing locations shifted by $>10$ k$\lambda$ and the amplitude of the oscillations differing by more than a factor of 2.

Although the ALMA observations allow for broad disk models that extend in toward the
central star, they are not consistent with a narrow ring model located far
from the star.  The contours for the inner and outer radius in Figure~\ref{fig:mcmc} show the absence of any models with large $R_\text{in}$ and small $R_\text{out}$, indicating that the disk must be broad.  Indeed, we can place a strong upper limit, $R_\text{in}<25$ AU with $99\%$ ($3\sigma$)
confidence.  Given the values of $R_\text{in}$ and $R_\text{out}$ from our best-fit model, the
fractional width of the $\tau$ Ceti disk is $\Delta R/R = 1.6^{+0.3}_{-0.6}$.
If we assume that the outer belt edge at millimeter wavelengths aligns
with the edge found at far-infrared wavelengths ($R_\text{out} = 55$~AU), we can place
a lower limit on the belt width, $\Delta R > 30$~AU.
 At $99\%$ confidence, $\Delta R/R > 0.75$.
 For comparison, our Solar System's classical Kuiper Belt has a fractional width of $\Delta
R/R \sim 0.18$ \cite[e.g.][]{hah05,ban15}, significantly more narrow.  In fact, the Kuiper Belt
appears to be confined between Neptune's 3:2 and 2:1 resonances.  Similarly, the Fomalhaut
debris disk appears narrow with $\Delta R /R \sim0.1$, possibly attributable to planets orbiting both interior to
and exterior to the ring \citep{bol12}.  In contrast, recent ALMA observations of
the HD~107146 debris disk \citep{ric15} indicate that its belt extends from
30~AU to 150~AU ($\Delta R/R \sim 1.3$), with a break at $\sim70$AU.
The $\epsilon$ Eridani debris disk also appears to be somewhat broader with a
fractional width determined from resolved SMA observations of $\Delta R/R = 0.3$ \citep{mac15b}.
The fractional width of the $\tau$ Ceti belt is
substantially larger than both the classical Kuiper Belt and Fomalhaut.
However, the $\tau$ Ceti belt is comparable in width to the HD 107146 disk,
suggesting that it might also have a more complicated radial structure,
which we are unable to resolve with these observations.

\cite{kal06} discuss the implications of the observed diversity in debris disk structures
in the context of scattered light observations.  For a narrow belt structure, both
the inner and outer edges of the disk must be maintained by gravitational perturbers
such as stellar or substellar companions, or be confined by mean-motion resonances with an interior
planet as is the case for our own Kuiper Belt.  Without any such confinement mechanism
for the outer disk edge, and since more massive planets have been ruled out around
$\tau$ Ceti at distances approaching $\sim10$ AU \citep{law14}, the expected structure is indeed a wide belt.

\subsection{Central Component}
\label{subsec:star}

In addition to the extended emission from an outer belt, the ALMA 1.3~mm image shows a bright, unresolved point source (see the constant positive offset on long baselines in Figure~\ref{fig:vis}) at the expected position of the star with a flux density of $0.69^{+0.02}_{-0.05}$ mJy.  For a G8.5V star with an effective temperature of $5344\pm50$~K, an extrapolation of a PHOENIX stellar atmosphere model \citep{hus13} predicts a 1.3 mm flux density of 0.60~mJy (with 5\% uncertainty).  Thus, the flux density of this central source is marginally higher than the expectation for the stellar photosphere at this millimeter wavelength.  We note, however, that an extrapolation of the mid-infrared flux of the star, as measured by WISE  at 22~$\mu$m \citep{wri10} and AKARI at 9 and 18~$\mu$m \citep{ish10}, yields a prediction for the flux of the stellar photosphere at 1.3~mm of $\sim0.5$~mJy, substantially lower than the measured 1.3~mm flux density.  Our ALMA measurement is complemented by previous observations by \cite{vill14} with the Karl G. Jansky Very Large Array (VLA) at 34.5~GHz (8.7~mm) and 15.0~GHz (2.0~cm).  At 8.7~mm, the measured flux density is $25.3\pm3.9$~$\mu$Jy, significantly higher than the predicted photospheric flux density of 14~$\mu$Jy.  While the star is not detected at 2.0~cm, a robust 99\% confidence upper limit is determined of $<11.7$~$\mu$Jy (model photospheric prediction of 2.5~$\mu$Jy).

\begin{figure}[ht]
\centerline{\psfig{file=fig6,width=14cm,angle=0}}
\caption[]{\small \emph{(left)} Flux density spectrum of $\tau$ Ceti from ALMA and VLA observations. The dashed line indicates the expected spectral index of 2.0 for a classical photosphere. \emph{(right)} Brightness temperature spectrum calculated assuming the photospheric radius of the star. For both plots, our ALMA measurements are shown as blue circles and the VLA measurements \citep{vill14} are shown as black diamonds.  Detections are indicated by points with $1\sigma$ error bars.  The 99\% upper confidence limit at 2.0 cm is indicated by the downwards arrow.  Again, the dashed line indicates the expected brightness temperature for a classic photosphere with the brightness temperature determined from our 1.3~mm ALMA measurement.
}
\label{fig:star}
\end{figure}

As \cite{vill14} discuss, the observed unresolved emission from $\tau$ Ceti at both millimeter and centimeter wavelengths plausibly arises from a hot stellar chromosphere.  Similar excess emission at long wavelengths has been noted for several neighboring Sun-like stars, including $\alpha$ Cen A and B (spectral types G2V and K2V, respectively) observed with ALMA by \cite{lis15} and $\epsilon$ Eridani (spectral type K2V) observed with the Submillimeter Array (SMA) and Australia Telescope Compact Array (ATCA) by \cite{mac15b}.  We combine our new ALMA 1.3~mm flux density with the previous VLA 8.7~mm measurement and 2~cm upper limit, and determine the Planck brightness temperature at all three wavelengths \cite[following][]{lis13}.  Figure~\ref{fig:star} shows the resulting ALMA and VLA constraints on both the flux density and the brightness temperature spectra of $\tau$ Ceti. We assume that the photospheric radius is comparable at optical and millimeter/centimeter wavelengths, and adopt a value of $0.793\pm0.004$ $R_\odot$, obtained from interferometric measurements using the FLUOR instrument on the CHARA array \citep{dif07}.  At 1.3~mm this analysis yields $T_B = 5,800\pm200$ K, modestly hotter than the effective temperature of $5344\pm50$~K.  However, at longer wavelengths, the brightness temperature diverges significantly from the photospheric prediction with $T_B = 9,300\pm1400$~K and $<23,000$~K at 8.7~mm and 2~cm, respectively.

Additionally, the spectral index at long wavelengths of the central emission from $\tau$ Ceti shows the same deviation from an optically thick photosphere (spectral index of $\sim2$) as is seen for $\alpha$ Cen A and B and $\epsilon$ Eridani.  Between 1.3 and 8.7~mm, the spectral index of the central peak in our observations of $\tau$ Ceti is $1.74\pm0.15$ (with the $\sim10\%$ uncertainty in the flux scale and the $1\sigma$ modeling errors added in quadrature).  For comparison, the measured spectral indices between 0.87 and 3.2~mm are 1.62 and 1.61 for $\alpha$ Cen A and B, respectively \citep{lis15}.

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

We observed the $\tau$ Ceti debris disk with ALMA at 1.3~mm with baselines that probe $1\arcsec$ (4~AU) scales.  These are the first observations of this nearby system with a millimeter interferometer and reveal somewhat patchy emission from a dust disk surrounding an unresolved central emission peak.  In order to characterize these two emission components, we fit simple parametric models directly to the visibility data within an MCMC framework.

Our best-fit model yields an inner belt edge of $6.2^{+9.8}_{-4.6}$ AU,
consistent with the analysis of previous far-infrared \emph{Herschel}
observations.  Given the relatively low sensitivity at short baselines in
the ALMA observations, we are unable to place a tighter constraint on the
inner edge and its position relative to the proposed five planet system.
These data, however, provide a strong lower limit on the fractional width of
the belt, $\Delta R/R > 0.75$ with $99\%$ confidence.  This result implies that
the $\tau$ Ceti debris disk is broad, much wider than the classical Kuiper Belt
in our Solar System and more comparable to the HD 107146 debris disk \citep{ric15}.

The bright central peak at the stellar position has a flux density of $F_\text{1.3mm}=0.69^{+0.02}_{-0.05}$~mJy, somewhat higher than the predicted flux of the stellar photosphere at 1.3~mm.  At longer centimeter wavelengths, this excess is more significant, increasing to $\sim2\times$ the photospheric prediction in VLA observations at 8.7~mm \citep{vill14}.  The spectral index between these two measurements is $1.74\pm0.15$, shallower than the expectation for an optically thick photosphere.  Given the high brightness temperatures at both 1.3 and 8.7~mm, this excess emission is likely due to a hot stellar chromosphere. Similar spectra have been observed for other nearby Sun-like stars, e.g. $\alpha$ Cen A/B and $\epsilon$ Eridani.

These first ALMA observations of the $\tau$ Ceti system allow us to probe the structure of the debris disk with higher resolution than previous work.  However, higher sensitivity observations at shorter baselines are still needed to constrain
the location of the inner edge of the dust belt more precisely.  If the disk extends in towards the star, within the orbit of the outermost proposed planet, this provides strong evidence against the posited five planet system.
However, if the disk inner edge is located well outside the proposed planetary system, an additional massive planet on a wide orbit may be required to clear out the central hole in the belt.  Additional observations with the ACA could provide the necessary sensitivity to determine the position of the inner disk edge and its implications for an interior planetary system.

\acknowledgements
This paper makes use of the following ALMA data: ADS/JAO.ALMA\#2013.1.00588.S.
ALMA is a partnership of ESO (representing its member states), NSF (USA) and
NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan) and KASI
(Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA
Observatory is operated by ESO, AUI/NRAO and NAOJ. The National Radio Astronomy
Observatory is a facility of the National Science Foundation operated under
cooperative agreement by Associated Universities, Inc. M.A.M acknowledges
support from a National Science Foundation Graduate Research Fellowship
(DGE1144152).  S.M.L. gratefully acknowledges support from the NRC Canada Plaskett Fellowship.
B.C.M. acknowledges support from a Natural Science and
Engineering Research Council (NSERC) Discovery Accelerator Supplement grant.
G.M.K. is supported by the Royal Society as a Royal Society University Research Fellow.
M.B. acknowledges support from a FONDECYT Postdoctral Fellowship, project no. 3140479 and the Millennium Science Initiative (Chilean Ministry of Economy), through grant RC130007.

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Stips ist eine nostalgische, deutsche Liebeskomödie aus dem Jahre 1951 von Carl Froelich, dessen letzte Inszenierung dies war. Gustav Fröhlich und Heli Finkenzeller spielen die Hauptrollen.

Handlung
Oberstudienrat Dr. Klaus Michael Dirkhoff unterrichtete einst als Kunstlehrer am Mädchengymnasium einer Kleinstadt. Durch seine unkonventionelle und direkte Art hatte der allseits beliebte Pauker bei seinen Schülerinnen, die ihn nur "Stips" nannten, ein Stein im Brett. Grundentspannt reagierte er auf freche Sprüche, Scherze und Streiche, und da er auch noch recht attraktiv ist, waren all seine Schülerinnen am Lyzeum natürlich verliebt in ihn. Die Schulzeit liegt lange zurück, und die Schülerinnen von einst sind ihrer Wege gegangen. Jetzt aber werden die erwachsenen und zum Teil bereits verheirateten Frauen von heute wieder zu den Mädchen von damals, denn eine frohe Kunde macht die Runde: Stips ist zurück in der Stadt!

Acht Jahre lang war er fort, doch die Gefühle von so mancher Stips-Bewunderin hat sich nicht verändert. Dr. Dirkhoff ist inzwischen verwitwet, und einige seiner Schülerinnen beginnen zu bedauern, dass sie nicht mehr frei sind. Der heißgeliebte Pauker von einst stiftet allein durch seine Anwesenheit bereits emotionale Verwirrung und lässt die weiblichen Hormone verrückt spielen, was sich höchst schädlich auf die Ehen der jungen Damen auswirkt, zumal manche von ihnen unverhohlene Stips nachstellen. Am Ende landet der attraktive Endvierziger ausgerechnet bei derjenigen Ex-Schülerin, die damals zu denjenigen gehörte, die sich bezüglich der Offenbarung ihrer Zuneigung zu ihm deutlicher als andere zurückhielten. Diese Frau, Regine Wülfing, in die er sich verliebt hat, wird, da ist sich Stips ganz sicher, seinen beiden Kindern, nunmehr Halbwaisen, eine gute Mutter sein.

Produktionsnotizen
Mit Stips beendete der 75-jährige Kinoveteran Froelich seine rund ein halbes Jahrhundert währende Tätigkeit für das deutsche Filmwesen. Der Mitte 1951 in Berlin und Umgebung gedrehte Film erlebte seine Uraufführung am 4. September 1951 in Düsseldorfer Alhambra-Kino. Die Berliner Premiere war am 27. November desselben Jahres. Gelegentlich wurde der Film auch unter dem Titel Pauker Stips und die verliebte Mädchenklasse vertrieben.

Alfred Bittins übernahm die Produktionsleitung. Die Filmbauten stammen von Hans Luigi und Werner Szneidereit.

Kritiken
In Der Spiegel war zu lesen: "Regisseur Carl Froelich beweist, daß man selbst als 76jähriger die Finger von Vor-Weltkriegsreminiszenzen lassen sollte."

Der Filmdienst urteilte: "Die nostalgische Geschichte aus der wilhelminischen Zeit ist der letzte Film des deutschen Kinopioniers Carl Froelich."

Einzelnachweise

Weblinks

Filmtitel 1951
Filmkomödie
Deutscher Film
Schwarzweißfilm

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Highest Rated SUV Consumer Reports Best Suv 2020
Best Small Luxury SUV 2020
Home»Cadillac»2020 Cadillac Escalade Release Date, Redesign, & ESV Price»2020 Cadillac Escalade Release Date and Prices
2020 Cadillac Escalade Release Date and Prices
The Cadillac line has been around for two decades. Currently, the line has produced four generations. The fifth generation, the 2020 Cadillac Escalade, will soon be released. If you are a fan of Cadillac, here we have something interesting for you. We will tell you about the soon-to-be-released Cadillac's design, engine, equipment, release date, and price.
2020 Cadillac Escalade Redesign
Let's start with the design. For its exterior look, the next generation Cadillac Escalade ESV will likely to have a similar look to its predecessor. This means that it will have an attractive yet bold look. Its front part will have well-designed headlamps with large chrome grille.
For the interior, it will be a spacious one. With its three rows of seating with standard leather upholstery, the new Cadillac will be able to comfortably accommodate up to 8 passengers. The second and third row can also be folded, freeing more space if needed. The dashboard will have an 8-inch display with the latest CUE infotainment system.
Engine Specs & Fuel Economy
What about the engine? The new Cadillac should come with the same engine as its predecessor, which is to say it will have a 6.2-liter, V-8 engine paired with a 10-speed automatic transmission gearbox for its base model. This engine is capable of generating up to 420 horsepower with 460 lbs-ft torque. It will also available with all-wheel drive and rear-wheel drive configurations. In terms of fuel efficiency, the rear-wheel drive model will have 14/23 mpg, while the all-wheel-drive model will have 14/21 mpg.
There is also a rumor that the upcoming Cadillac will also be available with another engine option. Supposedly, a 4.0-liter, V-8 engine paired with a 10-speed automatic transmission gearbox with both all-wheel and rear-wheel drive configurations will be available. Unfortunately, there is no further information about the performance of this engine.
The standard equipment for the upcoming New Cadillac Escalade will include the following
Apple CarPlay and Android Auto connectivity
Bose audio system (16 speakers)
OnStar (Wi-Fi and 4G LTE available)
Power front seats with cooling and heating features
Surround-vision camera
There is also additional equipment. For instance
Blind-spot alert
Rear-entertainment system
2020 Cadillac Escalade Release Date and Price
Now, let's talk about the release date and price. There is no exact date of the 2020 Cadillac Escalade ESV Release date but it will be released in the second half of this year. The good news is that it is possible that the release may happen earlier.
As for the price of the fifth generation Escalade, there is no official information about it yet. We expect the price to start around $75,000 for the base model, $99,000 for the best-equipped model and over $100,000 for the model with a new engine.
So far, these are what we know about the upcoming Cadillac Escalade Concept. The soon-to-be-released Cadillac will not differ significantly from its predecessor. That said, you can expect some new engines and novelties from the new model. What do you think?
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Since its original printing in 1952, the publication of the Handbook of Texas has been made possible through the support of its users. As an independent nonprofit, TSHA relies on your contributions to close the funding gap for the online Handbook and keep it a freely accessible resource for users worldwide. Please make a donation today to preserve the most comprehensive encyclopedic resource on Texas history. Donate Today »
AROCHA, SIMON DE
Jack Jackson
AROCHA, SIMÓN DE (1731–1796). Simón de Arocha was the eldest of fifteen children of Francisco and Juana (Curbelo) de Arocha, both Canary Islanders in Texas. He was born in San Antonio de Béxar seven months after the isleños arrived there. In 1752 he married María Ignacia de Urrutia; their union produced eight children. Like his father, who had served as city clerk and public notary, Simón held important administrative posts. He was a judge over distribution of public lands and later an alcalde. He also served as commander of the provincial militia, in which he was a lieutenant general. In this capacity he escorted the uprooted Adaesaños (see LOS ADAES) to the new Trinity River site of Bucareli in 1774. When Teodoro de Croix visited Texas in 1778, Arocha prepared a census report of the province for the new commandant general and his historian, Fray Juan Agustín Morfi.
Photograph, San Fernando Cathedral, where Simón de Arocha is buried, in San Antonio. Image available on the Internet and included in accordance with Title 17 U.S.C. Section 107.
Simón and his brother Juan obtained title to eight leagues of land north of the site of present Floresville in 1782. With this ranch, called San Rafael de Pataguilla, they and their kinsmen soon became leading cattlemen of the province. Simón was instrumental in forging a roundup agreement with the missions in 1787. Three years later he and other family members virtually controlled the local governing body, the cabildo. When they attempted to use their influence to obtain another ranch at the junction of the Guadalupe and San Marcos rivers, other stockmen lodged a vigorous protest and were supported by Governor Rafael Martínez Pacheco. The ensuing feud cost the governor his job. Don Simón died on July 29, 1796; his wife, on April 27, 1812.
During the revolutionary disturbances of the early nineteenth century, in which the Arochas were dedicated insurgents, most of their property was confiscated. With the coming of Mexican independence, however, Arocha's grandson José Ignacio managed to confirm title to the original Arocha grant.
Bexar Archives, Dolph Briscoe Center for American History, University of Texas at Austin. Jack Jackson, Los Mesteños: Spanish Ranching in Texas, 1721–1821 (College Station: Texas A&M University Press, 1986). Nacogdoches Archives, Steen Library, Stephen F. Austin State University; Dolph Briscoe Center for American History, University of Texas at Austin; Texas State Archives, Austin. Virginia H. Taylor, The Spanish Archives of the General Land Office of Texas (Austin: Lone Star, 1955).
Canary Islanders
Ranchers and Cattlemen
Handbook of Texas Online, Jack Jackson, "AROCHA, SIMON DE," accessed July 17, 2019, http://www.tshaonline.org/handbook/online/articles/far36.
Uploaded on June 9, 2010. Modified on June 30, 2016. Published by the Texas State Historical Association.


text:
Players Championship preview
What would you shoot at TPC Sawgrass under Players Championship conditions?
By Dean Knuth
Carlos Amoedo
You might have had the opportunity at some point to play a golf course that is the site of a PGA Tour event, and maybe played reasonably well. But what if you played that same golf course when it was prepared for tournament week? And what if that course was already renowned as one of the most difficult tests the game can offer?
We take you to Ponte Vedra Beach and the Stadium Course at TPC Sawgrass, site of the next week's Players Championship.
Go in knowing that the creation of the late Pete Dye is a headache for even the best players in the world. The tournament field typically averages about a half stroke to three-quarters of a stroke over par 72 for a round. Now put amateurs of varying handicaps on the same tees—7,189 to 7,245 yards—in tournament conditions with fast and firm greens and deep rough.
There's history here. Golf Digest has proved in various exhibitions that amateurs have a tough time on difficult courses in tournament conditions.
At the 2007 U.S. Open, Tiger Woods said that a 10-handicap couldn't break 100 that week at Oakmont. That prompted three Golf Digest U.S. Open Challenges, the first played the Friday before the 2008 Open at Torrey Pines South. Tony Romo, a 2.2 at the time, shot 84; Justin Timberlake (6.0) shot 98; and contest winner John Atkinson, an 8.1-handicap selected from 56,000 contestants, shot 114. The next year, the Challenge again preceded the U.S. Open at Bethpage Black, and the round took six hours and 21 minutes. This time the four low-single-digit handicappers were Ben Roethlisberger, who shot 81, Michael Jordan (86) and Timberlake (88). The 10-handicap contest winner, Larry Giebelhausen, shot 101. (Tiger had bet Jordan that Michael wouldn't break 92, and after the round, MJ proclaimed, "I don't take checks.") Before the 2010 U.S. Open at Pebble Beach, contest winner Peggy Ference shot 118, following Mark Wahlberg (97), Wayne Gretzky (100) and Drew Brees (102).
The December before that competition at Pebble, Golf Digest's David Owen, a 6-handicapper at the time, played the course from the tips and shot 50-50—100. In 2018, Owen, then a 7.9-handicap ("and rising") left Connecticut in the winter and played Sawgrass from the shortest tees and from the tips, shooting an 82 at 5,019 yards and a 111 from 7,245 yards.
RELATED: The 17th at TPC Sawgrass—An Oral History
More perspective: Before the 2009 Masters, Golf Digest asked me to form a team to assess Augusta National Golf Club's Course Rating after it had been lengthened more than 500 yards during multiple transformations over the previous two decades. Augusta National doesn't have an official USGA rating. The reason? Despite the fact that almost every member has a USGA Handicap Index from another club, Augusta National maintains its system for members only.
I estimated Augusta National's Course Rating that week at a formidable 78.1. I estimated the Slope at 137—high, but not off the charts. From the championship tees, most Bogey Golfers can't reach Augusta's long par 4s in regulation, but the fairways are relatively wide and the players can hit relatively short third shots into greens, minimizing many of the difficulty factors (water, bunkers, green targets, etc.). I estimated that a player with a Course Handicap of 0 could expect to shoot an 81, a 9 might shoot 91, an 18 would shoot 103 and a 36 approximately 125.
THE DANGERS OF SAWGRASS
In 1985, Golf Digest sponsored a contest to identify America's Worst Avid Golfer, with the final to be played at Sawgrass. Angelo Spagnolo, then 31, made a 66 at the 17th—including a three-putt—on his way to "winning" with a 257 for 18 holes. After a flurry of line drives at 17 splashed and seven more bounced over the green into the water, Spagnolo reluctantly agreed when his caddie suggested putting onto the green from the adjoining walkway.
So what would you do at Sawgrass? Let's run some numbers.
Course Rating is a measure of a course's difficulty level for a scratch golfer—someone who has a 0.0 Handicap Index.
Slope Rating measures the relative difficulty of a course for Bogey Golfers and other players of "varying abilities" when compared with the Course Rating. Though there are no limits for a Course Rating—the par-73, 8,325-yard Pines Course at The International in Bolton, Mass., has a Course Rating of 80.0—Slope Ratings basically range from 55 to 155. Standard playing difficulty is 113.
At the Stadium Course at Sawgrass, the Course Rating issued by the Florida State Golf Association is 76.4 and the Slope Rating is 155. These are ratings for normal playing conditions—so the actual uncapped Slope Rating during the Players would be higher. On a non-tournament week, the average scores for scratch golfers would be in the area of 2.6 strokes over the 76.4 Rating, but under tournament week conditions I estimate the average score as close to 81 by a scratch player. A golfer with an 18-handicap typically would shoot 116, but would be in the 122-124 range under tournament conditions (see accompanying chart).
Rough and slicker greens during tournament week mean almost every hole demands forced carries over water or bunkers—a major challenge for amateurs when compared to pros. Also, some of the greens have a shallow depth, and most of the greens have severe slopes punishing you if you don't stop the ball near the hole, producing more three-putts than normal. Amateurs are challenged to produce the ball flight and spin needed to approach the greens correctly.
RELATED: Nine things to know about TPC Sawgrass
Adding to the challenge of the approaches, many fairways run at angles and then into pine straw, water and sand, causing amateur golfers to struggle with distance control and accuracy. Even a scratch golfer would expect to frequently score an 85.
Producing many double bogeys are four long par 4s—the 471-yard fifth hole, the 451-yard seventh, the 481-yard 14th and the 470-yard 15th—and, of course, the famed 137-yard 17th. A group of 36-handicappers who want to see the back tees that week, besides taking an extra hour or more to finish, would see scores over par almost double their handicaps.
HOW FAR DO YOU REALLY HIT IT?
Finally, let's discuss the ability of amateurs to get to the greens in close to regulation from the back tees. A study that I did for Golf Digest a number of years ago produced one of the most telling numbers in how far amateurs are behind pros' 300-plus-yard drives and how dramatically amateur players inflate their driving distances. In that test, lower-handicappers claimed their average drives went 247 yards, but driving distance stats taken in a pro-am tournament measured 232—a 15-yard exaggeration. Poorer players claimed a driving average of 227 yards but hit it 198 yards—a 29-yard exaggeration. The worse the players, the more they kid themselves about how good (and long) they are. Nobody, it seems, wants to admit he drives the ball less than 200 yards. Succumbing to self-delusion, it seems most amateurs tend to equate their best drive with their average drive. In looking at the self-assessed strengths and weaknesses from the amateurs who hit a fairway and then missed a green, "driving" was named a strength as often as it was a weakness.
It all adds up to a long and exhausting day for amateurs and a new appreciation for just how good PGA Tour pros really are—especially Rory McIlroy's winning rounds last year of 67-65-70-70 for a 16-under-par 272 total. That score would be out of reach for almost all amateurs even with handicap strokes.


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With sales doubling monthly, Lyst picks up $5 million to grow its 'social commerce platform'
by Alex Wilhelm — in Insider
Lyst, a self-styled 'social commerce platform' has taken on a $5 million Series A round of funding led by DFJ Esprit, and participated in by Venrex, Accel Partners, and Alex Zubillaga. Zubillaga's other investments include ChartBeat, Yipit, and Listia.
According to the company's release, it has doubled its sales each of the last three months. Thinking mathematically, that would put its revenues at roughly eight times their April level.
Lyst is an online fashion play. Aimed at the digitally savvy, the website lets users 'follow' brands, designers, and other elements of the fashion world. Updates are sent to users when certain items go on sale. Each user has a 'stylefeed' into which their content is placed. For those interested in clothing and its world on a day-to-day basis, the product is likely a welcome tool.
How Lyst makes money isn't hard to understand. From its website, describing how its features: "Search and shop from all of your favorite stores in one place and get instant sales alerts on products saved to your lyst."
That's actually somewhat elegant, when you combine it with the system of alerting users about sales: it has a perfect pull mechanism to feed its sales system. Someone else puts on a sale, and Lyst profits from it. According to the company, the money is set to be used to boost its relationships with fashion houses, and to build out its product.
How long Lyst can continue doubling its revenue is impossible to discern, but if the company can keep up that sort of revenue growth it will quickly become a staple in the fashion world.
Top Image Credit: Sebastian Dooris
Read next: Boulder startups band together, raising funds for wildfire relief efforts


Diet-friendly, no flour, no gluten, no guilt. I have no intention of claiming that cauliflower crust is a perfect imitation of classic pizza dough with flour and yeast. It's different. And it's better.
Heat the olive oil, add onion and garlic and cook until soft and golden.
Add tomatoes, season with sugar, salt and pepper. Bring to boil.
Simmer over medium heat until the sauce thickens (30-40 minutes), stirring every now and then.
Using a food processor, blend cauliflower florets until pureed. Lightly steam the cauliflower for 3-4 minutes. Set aside and let cool.
Use a cheesecloth to squeeze the excess water from the cauliflower.
Transfer to a bowl and combine with parmesan, mozzarella and a whisked egg.
Spread the "dough" into one large pizza on a parchment-lined baking sheet.
Top the pizza with tomato sauce, cherry tomatoes and mozzarella slices. Bake for another 10 minutes.


Like most dating apps, this one won't do you any good if it's not a popular app in your area. As successful as it is at forming long-distance relationships and successful marriagesTinder has long been accused of changing dating into some form of hookup game. But such small expense can greatly improve your chance to connect to the right person, whom you may fall in love with, on the site. You can buy coins as in-app purchases. It boasts over 40 million people although we're not sure how many of those are daily active users.
5. Free Dating App & Flirt Chat - Match with Singles BMAW Dating App: Black Men Asian Women Dating Mingle - Online Dating App to Chat & Meet People. Check out our top dating, hook-up and meet-up apps that will help you find but the mobile Internet has put almost every single person in your.
MANILA, Philippines – "Swipe left. But with dating apps now a dime a dozen, how do you know which one's best for you and your *ahem*.
Online dating site with free. Meet new website in the philippines dating in your matches for the list of american adults have the philippines mobile dating.
The option may especially work well for some pretty Filipina women. They help give you more visibility and features.
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You can even send a song or message users before or after they match with you.
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Here are the best dating apps for Android. It does so with varying degrees of success depending on where you live.
Looking to meet high-quality Filipino women online? These 6 popular Philippine dating sites and apps are the best place to start!.
your standards, it is like a mobile blind date, and I mean literally, because the platform They would be using the Messenger App as a means of chatting and if a boy or a girl I believe it is the most used dating application in the Philippines. With a remarkable member base of over million (and growing) and with a promise of introducing you to beautiful Filipino women from all around the world.
However, Zoosk pulls a fast one with their app.
Mobile dating apps philippines As a free member, you can communicate with paid members, but not other free members.
Just shake your phone to undo your rogue swipe. Introducing the convenience of the philippines?
The worst part of Zoosk is that there are two potential paywalls. MeetMe is another one of those location-based dating apps.
She'll have 24 hours to do so and then the man will have 24 hours to reciprocate.
Then the real fun begins. Filipinocupid android and paid.
Coffee Meets Bagel is one of the more popular dating apps out there.
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Vevo Partners with Apple to Stream iTunes Festival from SXSW
Tuesday March 11, 2014 10:35 AM PDT by Kelly Hodgkins
Music video and entertainment platform Vevo announced today that it is partnering with Apple to stream this week's iTunes Festival at SXSW. Apple is limiting the service to include the same streaming options offered by its own iTunes Festival coverage, which includes iOS devices, Macs and the Apple TV.
Starting Tuesday, March 11 and ending Saturday, March 15, viewers can launch the Vevo iOS app or open the Apple TV channel to watch live performances from ACL Live at the Moody Theater in Austin, Texas. Mac owners can view the live stream by pointing their Safari browser to Vevo's iTunes Festival website.
Three performances are scheduled each night, with headline acts to include major artists such as Coldplay, Kendrick Lamar, Soundgarden, Pitbull an Keith Urban. Select performances will be available for on-demand viewing after the concert is over.
iOS owners who prefer not to use Vevo can watch the daily concert series via Apple's iTunes Festival app [Direct Link], while Apple TV users can open the recently updated iTunes Festival channel. Both sources allow users to live stream the concert's shows as well as view concert lineups, on-demand performances and artist information.
Vevo is available for the iPhone [Direct Link] or the iPad [Direct Link].


Energy-conscious sailors worldwide are exchanging their incandescent bulbs for LED lights. LEDs work well in many applications, but some sailors find the beam they cast is too diffused to clearly spot distant objects. Pelican's Stealthlite Rechargeable 2460 uses a rechargeable NiMH battery pack to power its strong, focused LED beam. It should allow you to spot buoys or telltales, and it's fully waterproof, too.


The United States risks losing its AAA credit rating from Fitch if any deal to raise the legal borrowing limit does not include a plan to put public finances on a more sustainable footing, the ratings agency said Tuesday.
Fitch has long warned that a repeat of the 2011 debt ceiling crisis would result in a formal review of its AAA rating on U.S. sovereign debt. While it expects Congress to raise the debt ceiling -- making the risk of a U.S. default extremely low -- the nature and timing of the agreement will be critical.
"In the absence of an agreed and credible medium-term deficit reduction plan that would be consistent with sustaining the economic recovery and restoring confidence in the long-run sustainability of U.S. public finances, the current negative outlook on the 'AAA' rating is likely to be resolved with a downgrade later this year even if another debt ceiling crisis is averted," it said in a statement.
The Treasury Department said Monday it will run out of ways to keep the U.S. under the $16.394 trillion ceiling sometime between mid-February and early March. It takes in about $100 billion less in revenue every month than it has committed to pay to contractors, Social Security recipients, federal workers and debt holders.
Since the start of the year, it has been forced to resort to "extraordinary measures" to generate $200 billion to cover short-term borrowing needs.
The last time Congress negotiated an increase in the debt ceiling, in August 2011, the talks went down to the wire, bringing the U.S. close to the point of being unable to meet its financial commitments. Markets took fright and Standard & Poor's cut its rating on the U.S. to AA+ from AAA.
Congress must also decide on the fate of spending cuts deferred under the Jan. 1 deal that averted the "fiscal cliff" at the turn of the year, and renew the federal government's spending authority, due to expire March 27.
Fitch said Tuesday another round of last minute short-term fixes would perpetuate the uncertainty over tax and spending, and fail to place U.S. finances on a sustainable path in the medium term.
In the absence of a higher debt ceiling -- and assuming the sale of gold reserves or minting platinum coins are non-starters -- the Treasury Department will have to start delaying payments as they fall due.
Fitch said that would equate to a squeeze twice the size of the "fiscal cliff", and there was no assurance the U.S. could prioritize debt service payments over its other commitments.
"Arrears on such obligations would not constitute a default event from a sovereign rating perspective, but very likely prompt a downgrade even as debt obligations continued to be met," it added.


Kevin Clark Originals Ocean Lighting products bring the beauty of the ocean sea creatures to your living environment. From Bronze Dorado & Big Game Fish to Turtles, Shells and Sea Reef Detail. Our Ocean Lighting is functional art work that can be enjoyed at your home, office or yacht. The choices are endless and as deep as the sea!


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Adult Language Program
1,600 Hours to create Intermediate Speakers
The four-year program built upon years of grassroots revitalization work and created a unique collaboration between Syilx Nation governments, bands, partner organizations, and community members to support a language house for young adult learners. Eight new speakers graduated from the program in June 2019.
Immersion Methods
The adult class met two days a week for FOUR years and studied Nsyilxcn Curriculum developed by Paul Creek (Salish School of Spokane) and their proven fluency model.
The highly motivated young adult learners were supported by Bands and workplaces.
Our partner organization, the Salish School of Spokane, is the inspiration for our efforts. They currently have twenty advanced Nsyilxcn learners and teachers and operate a full-time immersion school to 75 children, a hub of adult fluency, and a community of new speakers and families.
Sʔímlaʔxʷ has generated several peer reviewed research articles throughout this work. Her PhD thesis is here.
Filmed assessments were posted during the Chopaka Language House project, 2011, and the Tlingit revitalization project (video #1, video #2).
Elder Involvement
Elder recordings are listened to each day and Elders visit and provide immersion each month.
As a component of in-class learning and homework, students learn to edit transcriptions.
SLH generates advanced literature and documentation with Elder speakers. Documentation meets a critical need to record our precious remaining Elders.
Five hours (50 stories) of stories are recorded, transcribed and shared each year. Books and audio are shared with Bands, students, libraries, schools, on this website, and the Sncәwips Museum site.
We deliver a four year, 1,600 hour, program using a proven curriculum and intensive immersion. Our first cohort of 12 adults started in September 2015 and graduated in June 2019. Students were supported by Bands and employers to attend classes two days a week for FOUR years. We deliver the Nsyilxcn Curriculum developed by the Salish School of Spokane (Paul Creek), and learn by recording and transcribing Elders. The learning is transformational. Beginners transformed into intermediate speakers and a new generation of teachers.
We record Elders, publish advanced language materials, raise awareness, and lobby for larger cohorts of successful programs across our Syilx Nation.
Speaking assessments are filmed each year and shared on YouTube. After 200 hours students transformed from low-beginner to mid-beginner speech; after 1,000 hours they achieved high-beginner/low-intermediate.
Envisioning a Future of Speakers
Imagine a meeting in one of our member communities four years from now —there is an ongoing land title discussion in the court system. Someone is needed who can speak to the land-based messages embedded in our captíkʷł story system in order to prove rights and title within unceded Syilx territory. A young, well-dressed, articulate woman steps up, a recent graduate of the Syilx Language House. She is 25 years old and completed her Bachelor's degree in Indigenous governance and law while studying in the language house.
She says, "I am able to do this."
During her time in the Language House she learned to speak Nsyilxcn at a mid-intermediate level, record and transcribe Elders, archive materials, become a language advocate and spokesperson, intimately connected with Syilx story systems and deeply embedded language-based truths.
kʷu kłsqiʔs. We have a dream.
It is our dream that this story will be brought to life with the language tools being taught to our students today.


Henry Kitchen and Bath is proud to present this decorative bathroom light, by Robern. The PL3.540TLSC82D4 is made from premium materials, this Bathroom Light offers great function and value for your home. This fixture is part of Robern's decorative Profiles Lighting Collection, so make sure to check out other styles of fixtures to accessorize your room.


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» Gun ordinances face defiance from law officers
The head of a nationwide sheriffs coalition is calling on Vermont's law enforcement officers to defy three controversial gun control measures …
We're seeing sheriffs in New York oppose the Safe Act and Gov. Cuomo …
Sheriffs in Colorado are refusing to enforce that state's new background checks and ban on high-capacity magazines. In Connecticut, tens of thousands of residents are refusing to comply with a new state law that requires registration of guns and high-capacity magazines. In Saratoga Springs, N.Y., citizens publicly protested the state's new SAFE Act last week by burning a thousand gun registration forms.
In Vermont, hundreds – some blazoned in orange hunting attire and hoisting the Gadsden Flag – rallied at the state Capitol to urge the Legislature to uphold Vermont's strong Second Amendment gun laws
» Mom Dupes Replacing Mayor Dupes
We've already been told that Moms Demand has "merged" with MAIG. But did you know that they've finally announced that they are just a "campaign" of MAIG?
The billionaire gun hater and scold demands that we give up our guns. He saw a "stay at home mom" and former corporate communications executive for Monsanto running a Facebook page against guns and thought to himself, "My anti-gun mayors are getting put in jail. My other mayors are realizing that by 'illegal guns' I actually mean 'all guns' and are abandoning me. I could give these women some of my petty cash and spend the rest of my life hiding behind their petticoats."
The money that Nanny Bloomberg paid for Moms Demand was money well spent, because without at least the appearance of grass roots, even their media allies will have to admit that it's just an obnoxious billionaire trying to impose his will on the rest of us.
» Dick's Sporting Goods Now Discriminating Against Law-Abiding Gun Owners
It wasn't that long ago when Dick's Sporting Goods pulled all black semi-automatic rifles from their shelves. They felt that in light of the Sandy Hook tragedy, these guns possibly should not be sold. This of course caused massive complaints against Dick's, by law-abiding gun owners protesting their lunacy.
Dick's has now returned for round two!
Where the parking lots are free of patriot shadow
Joe Biden delivered an emotional plea for more gun laws at Western Connecticut State University, taking the stage with Gov. Dannel Malloy and telling listeners, "We have to speak for those 20 beautiful children who died" at the elementary school.
"Then suddenly," Burgess said, "the bill passed with emergency certification. Nobody read it. [Lawmakers] got the bill and then overnight they passed it. A hundred thirty pages, nobody even had time to read it."
The state has warned the estimated 325,000 to 350,000 residents who need to register their weapons that the penalty for noncompliance is arrest.
In one recorded telephone call to Connecticut State Police Lt. J. Paul Vance, a woman who gave her name only as Ashley is heard asking for clarification about the fate of her husband, who failed to register his weapon by the deadline.
The conversation spanned about seven minutes and ended abruptly when Ashley said, "You're the servant, we're the master," and Vance cut her off, saying: "I'm the master, I'm the master, Ma'am."
That sentence should have been followed by a ratchet sound and click just behind his pompous tyrannical head.
Another policeman, Branford officer Joseph Peterson, was placed on paid leave pending the outcome of an internal investigation about Facebook postings he made in response to citizens who wanted to know what he'd do if they didn't turn in their guns.
Replying to a resident who asked if police would confiscate weapons from homeowners, Peterson replied on Facebook: "It's not a Nazi policy, you thick-headed idiot, it's a state statute, OK, I don't come to your job [to] tell you how to do yours."
» McConnell just cut the legs right out from under House Republicans…
Cruz, Lee, Paul, Enzi, and Roberts were all standing together to strip the IMF legislation out of the aid package bill for Ukraine. As I said earlier, the IMF legislation would basically double the contribution of the US to the IMF fund while lessening America's influence over how that money is spent.
So what does McConnell do? Does he stand with the filibuster effort?
OSHA Taking Orders from Union Thugs
» SEIU Uses Federal Inspections to Target Houston Small Business
Union organizers are showing up at Occupational Safety and Health Administration (OSHA) inspections of an open-shop business that has been targeted by the country's second-largest union.
» Union representatives join federal government safety inspectors on site visits to non-union businesses
"By allowing outside union agents and community organizers access to nonunion employers' private property, OSHA is injecting itself into labor-management disputes and casting doubt on its status as a neutral enforcer of the law," Baskin testified.
OSHA did not return a request for comment. SEIU declined to comment.
» Obama Kills Tomahawk, Hellfire Missiles, Spends Millions on Green Energy
The world is looking very peaceful these days. What are the odds that we'll need a Navy anyway? Cruise missiles are outdated like bayonets and horses.
Advanced technology involves promising Putin to be super extra flexible when he invades Poland while blowing the military budget on Green Energy …
That happens to be neither green nor energetic.
The Tomahawk missile program—known as "the world's most advanced cruise missile"—is set to be cut by $128 million under Obama's fiscal year 2015 budget proposal and completely eliminated by fiscal year 2016, according to budget documents released by the Navy.
In addition to the monetary cuts to the program, the number of actual Tomahawk missiles acquired by the United States would drop significantly—from 196 last year to just 100 in 2015. The number will then drop to zero in 2016.
The Navy will also be forced to cancel its acquisition of the well-regarded and highly effective Hellfire missiles in 2015, according to Obama's proposal.
At which point peace on earth will break out.
» Al Sharpton, Democrats, honor woman convicted of voter fraud
» NYT reporter: Obama administration 'the greatest enemy of press freedom' in a generation
» AMERICA DESERVES BETTER THAN CLINTONS
» 26 potentially insightful and undoubtedly offensive quotes from Greg Gutfeld's new book 'Not Cool'
"…in any place where something isn't cool, you will see these three words strung together: "old white men."
"The definition of cool: popularity without achievement. It's how President Obama got the youth vote."
To the cool, empathy is "deep." It's "challenging." To a tougher, more realistic past America, it was "bull*hit."
"Fact is, the desperate desire to be cool has skewed our culture toward nihilism, carelessness, and ineptitude. It is now cool to be an idiot. A jackass. It's cool to be a failure, as long as your failure is the basis for a reality show. And on the reality show you can do what's considered ultimately cool: "raise awareness."
"Facebook paid no income taxes for 2012 … because this company happened to be Facebook, the story was a one-day affair. … If this company were something that actually made something in a factory or field, it would be roundly condemned by every single media hack on the planet."
» Muslim Sex-Offender Who Tried to Kidnap 4-Year-Old Girl Excused for "Cultural Differences"
The Muslim sex offender, was not deported or locked up after his previous offenses. Now he's been kept free once again because of "cultural differences."
Why don't we call the cultural differences excuse what it really is? Muslim Rape Privilege.
» Sharia Compliant Wills Hit Britain for 1st Time: You Think It Can't Happen Here?
For all we hear about the Islamization of Britain, a 'first' has just occurred.
Under ground-breaking guidance, produced by The Law Society, High Street solicitors will be able to write Islamic wills that deny women an equal share of inheritances and exclude unbelievers altogether.
The documents, which would be recognised by Britain's courts, will also prevent children born out of wedlock – and even those who have been adopted – from being counted as legitimate heirs.
Anyone married in a church, or in a civil ceremony, could be excluded from succession under Sharia principles, which recognise only Muslim weddings for inheritance purposes.
» THE CARBON DIOXIDE LEVEL IS DANGEROUSLY LOW
"Global warming" is an irrational belief whose proponents demonstrate no interest in examining scientific evidence that may prove their beliefs incorrect. As a simple cult, it has failed to progress much beyond the concept of original sin, apocalyptic visions, sumptuary laws, and the selling of indulgences. Wind farms are the temples of this state-sponsored belief system. This cult doesn't extend to building aged-care homes, hospitals, or anything much for the common good. Instead it degrades the fabric of society by misdirecting human effort. Its true believers can hardly be blamed; the global warming cult is not much different from any of the other end-of-the-world cults that have preceded it.
Once again, American taxpayers are the wind beneath Michelle Obama's wings – this time flying her to China, along with every female member of her immediate family except Barack.


Are you a non-Canadian who has been offered a faculty appointment at Queen's University?
To start your new appointment you must first obtain the appropriate official documentation to enter Canada and to begin working at Queen's University. Usually,a Labour Market Impact Assessment is required. This will be initiated by Queen's and documentation will be forwarded to you.
For individuals under the exempt categories, Queen's will complete an "offer of employment" online and pay a $230 "employer compliance fee" to Immigration, Refugee and Citizenship Canada (IRCC). The system provides a personalized ID number which will be forwarded to you and must be inserted into the work permit application.
Where can you get help in your language to ensure your application is complete?
Where can you find out if you might be inadmissible to Canada?
Review the web links to the Citizenship and Immigration website that will help you answer these questions under First Steps to Immigration.
Carefully read and follow all documentation you receive from Queen's and Citizenship and Immigration Canada. If you have questions about starting at Queen's, contact the Faculty Recruitment and Support Program.
As per your letter of appointment, it is your responsibility to maintain your immigration status by initiating, as soon as possible after taking up your appointment, an application for Permanent Resident status.


Strawberries, ice cream, music – enjoy a Sundae for Good this November!
Why strawberries and ice cream? Strawberries celebrate life – they're a super food and are a symbol of summer – what's not to love? The Mary Potter Hospice Strawberry Festival helps us raise between $40,000 to $60,000 across our three festivals, plus helps to raise awareness of Mary Potter Hospice. Please keep Hospice free for our community and support our strawberry festivals this November.
Strawberry sundaes will also be available for pre-order! Purchase online to pick-up from Midland Park or you can get them delivered for free to a Wellington CBD address thanks to DeliverEasy.
Kāpiti Primary School, Corner Rimu and Kapiti Roads, Paraparaumu, Kāpiti Coast. Gold coin donation on entry. The Kāpiti Coast Festival has so much on for all the family – strawberries and ice cream (of course!), Kāpiti's best food trucks, face painting, burgers/sausage sizzle, bouncy castle, kids entertainment, plant sales, linen sales and entertainment throughout the day on the big stage.
Join us for the 13th annual Mary Potter Hospice Strawberry Festival at Midland Park and enjoy a Sundae for Good! As well as strawberry Sundaes for Good (thanks PAK'nSAVE Kilbirnie!) there'll be chocolate dipped strawberries, live music, a pop-up strawberry themed op-shop and our amazing corporate volunteers ready and waiting to serve you up your delicious Sundae for Good – all for $6 each!
Do you live around Porirua? Make sure to drop by PAK'nSAVE Porirua for our sausage sizzle and strawberries and ice cream.


Northern Illinois & Wisconsin Railway Corporation, doing business as NIWX Corporation, is a locomotive leasing, finance and equipment management company founded in 1999. NIWX sells and leases low horsepower General Motors Electro-Motive Division (EMD) switcher and road switcher locomotives, General Electric (GE) road-switcher locomotives, and Caterpillar re-engined switcher and road switcher locomotives. Locomotives are inspected, reconditioned as necessary, fully qualified and are in excellent condition.
A service provider of your choice, and can be tailored to your requirements.
Our number one goal is customer satisfaction; our aim is to exceed your expectations. Please contact us for more information.


Dave Contarino, President of Contarino & Associates LLC, is a powerhouse political consultant for the Democratic party.
Dave Contarino is a political strategist and business consultant based in Louisville, Kentucky. Dave Contarino has more than 25 years' experience in political campaigns. As a former high-ranking government official, Dave Contarino believes that living in the real world (outside of Washington, D.C.) makes for a better political consultant.
Too many consultants live "inside the beltway," in the supercharged world of Washington, D.C., consuming and trading political news and gossip all day long, says Dave Contarino. Even the best can lose touch with the day-to-day realities of citizens whose votes they seek to influence.
Dave Contarino feels fortunate to live on one of the most beautiful lakes in Kentucky. Known for its diverse fishing, the Herrington Lake area is just a short drive from Lexington, Kentucky, where it regularly attracts visitors from throughout the South. From his cabin, Dave Contarino enjoys beautiful views and some of the best fishing in the area, which provides a welcome break from his hard-hitting work as a political consultant.
Dave Contarino loves to talk about the place he calls home on many weekends and lazy summer days. Below he answers questions about some of the best features of Herrington Lake.
Dave Contarino, who has built a steady career as a respected political consultant, spends much of his free time skiing. While his current hometown of Louisville, Kentucky, doesn't allow easy access to his favorite pastime, Dave Contarino schedules frequent getaways to his favorite ski town: Taos, New Mexico.
A 15-year resident of Santa Fe, Dave Contarino is familiar with the benefits of the Taos area, which is known for both its history and culture. Below, he answers a few frequently asked questions about the history of his favorite ski town, which he visits as often as possible.
Connect with Dave Contarino on Facebook, Twitter, Linkedin, Google Plus and Pinterest.


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Artist Spotlight: LIMBS
Articles by Shane McCarron August 7, 2018 August 7, 2018
The Vans Warped Tour, as we knew it, was laid to rest this past weekend after 24 cross-country summer tours. It came to its conclusion in hot & sticky Florida as fans waited out lightning delays, moshed through mud, and powered through the Florida Warped Tour heat to see their favorite bands.
I attended the Tampa date on Saturday (still sad it wasn't at Vinoy Park in St. Pete) and I had one of my favorite Warped Tour experiences of all time. The lineup was stacked on all stages as we saw Warped Tour legends such as Every Time I Die, Less Than Jake, and Reel Big Fish. The crowd was full of energy even with the 90+ degree heat all day long.
One of my favorite things about the Vans Warped Tour is their commitment to showcasing up and coming bands. The Full Sail stage was home to so awesome on the rise bands and even local talent. My Spotlight Band from the 2018 Vans Warped Tour is LIMBS. They're a post-hardcore band from Tampa, Florida and they we're an eye and ear opening start to the day. From start to finish LIMBS showed the passion and intensity of what it means to play in front of a hometown crowd.
LIMBS released their first EP (with their updated lineup) back in 2014 titled 'Admission' which received heavy praise. In 2015 they released a pair of singles and they rapidly gained attention in 2016 as they toured with Saosin. In 2017, LIMBS released a six track EP titled 'SLEEP' which was their debut release on Equal Vision Records and it was also produced by Tim McTague from Underoath, they toured with Envy as well as Hail the Sun. 2018 has been a massive year for LIMBS, they joined Tampa Post-Hardcore legends Underoath on their No Fix tour. They also released their first full length album titled 'Father's Son' and it is quite the debut record.
After playing two of the Florida dates for Vans Warped Tour, LIMBS will enjoy a quick tour with Emery and Oh, Sleeper to finish off August. Expect big things from this band in the near future.
Keep up with LIMBS: Apple Music // Facebook // Instagram // Spotify // Twitter
Phish at The Gorge: A 3-Day Phiesta
This Atlanta-based Festival is Beyond Your Wildest Imagination


Included below are homes for sale in Spencer County, Kentucky, updated daily from the Greater Louisville MLS. If you would like more information on any of these Spencer County ky real estate listings, just click the "Request More Information" button when viewing the details of that property. We can provide you with disclosures, past sales history, dates and prices of homes recently sold nearby, and more.
And, if you haven't already, be sure to register for a free account so that you can receive email alerts whenever new Spencer County homes for sale come on the market.


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redpajama_set_name: RedPajamaGithub


You will Watch Aqua Teen Hunger Force Season 2 Episode 22 online for free episodes with HQ / high quality. Stream cartoons Aqua Teen Hunger Force Episode 22 The After Master Shake nearly destroys the house by leaving garbage everywhere (especially in Frylock's room, whose entrance he has bricked closed), burning styofoam, stockpiling chicken carcasses, and planting land mines in the hallway, Frylock becomes disgusted and moves to a condominium. Frylock throws a housewarming party, but none of the people he invites attend. Out of desperation, he invites the Mooninites, who show up only long enough to trash his place.


Fine Art Print named "Exceptional Rose" digital artwork by Lea Schock, Canvas Print.
This outstanding still life was created as a gift for exceptional events , printed on Canvas, stretched on wooden frame, quality checked and signed manually by the artist.
... the birthday present for my girlfriend. She was overwhelmed, because she loves roses, and she is one! The package came right in time! thank you!