text:
\section{INTRODUCTION}
Widespread strong turbulence is an outstanding characteristic of the molecular clouds (MCs) in the central molecular zone (CMZ) of the Milky Way.
Their velocity dispersions lie about a factor of 5 above the size--velocity width relationship for the Galactic disk, irrespective of choice of tracer lines \citep{Miyazaki2000,Oka2001a,Shetty2012a}.
The virial parameters ($\ifmmode{\alpha_{\rm vir}}\else{$\alpha_{\rm vir}$}\fi$) of the CMZ clouds are systematically $\sim 10$ times those in the Galactic disk, indicating that they are not self-gravitating but likely bound by external pressure \citep{Miyazaki2000,Oka2001a}.
{\bf
It is suggested by many authors that the high degree of turbulence in the CMZ may affect the star formation process there.
Primarily, the strong turbulence suppresses the star formation rate (SFR) because the gravitational collapse of dense clumps in the MCs is slowed or inhibited by the high turbulent pressure.
Several recent works suggest that the SFR within the CMZ may be suppressed by this effect to a value 1--2 orders of magnitude lower than the value expected from its dense gas mass \citep{Longmore2012b,Kruijssen2014}, although other effects such as the tidal shear, strong magnetic field, and enhanced cosmic-ray flux may also play significant roles in determining the SFR \citep{Yusef-Zadeh2007,Kruijssen2014}.
Meanwhile, turbulence may also facilitate the formation of massive stars and stellar clusters in sites of cloud--cloud collision \citep{Habe1992,Inoue2013a}.
This collision-induced star formation is a popular explanation for the highly active star formation in the Sgr B2 complex \citep{Hasegawa1994}, and there is increasing evidence suggesting that cloud--cloud collisions play a key role in cluster formation in the CMZ \citep{Higuchi2014} as well as in the Galactic disk region \citep{Furukawa2009,Higuchi2010a}.
}

The properties and origin of turbulence in the CMZ are, however, yet to be fully understood.
{\bf
\cite{Shetty2012a} show that the size--linewidth relationship holds both within and among the CMZ clouds over an order of magnitude in the spatial scale.
This indicates that the turbulence driving in the CMZ is predominantly a large scale one, which is consistent with the idea that the turbulence is maintained by interactions with frequent supernova explosions \citep{Shetty2012a} or with the bar potential in the inner Galaxy \citep{Rodriguez-Fernandez2006}.}
Meanwhile, high spatial resolution surveys in millimeter and submillimeter carbon monoxide (CO) lines \citep{Oka1999,Oka2012}\ detected a considerable number of small clumps with extremely broad velocity widths inconsistent with the size--velocity width relationship;
their velocity widths are 40--120 $\kmps$ in full width at zero-intensity (FWZI) in spite of their small spatial sizes of approximately 1--3 pc in radius, indicating enhancement in velocity widths by a factor of 4  from the size--linewidth relationship \citep{Tanaka2014}.
{\bf
These clumps are distinguished by their spatial compactness from the larger-scale broad-line structures of a few 10 pc in sizes that were identified by \cite{Bania1977} and \cite{Liszt2006} at larger Galactic longitudes ($|l|>1^\circ$).
}
The recent CO \JJ{3}{2}\ survey with the ASTE 10-m telescope \citep{Oka2012}\ identified 70 such high velocity {\bf dispersion} compact clouds \citep[HVCCs;][]{Oka2007} and HVCC-like features, most of which were not associated with known energy sources for driving such small scale turbulence.

Recently, we reported results of the HCN \JJ{4}{3}\ mappings obtained with the ASTE 10-m telescope toward the Sgr C complex, which include one of the most prominent HVCCs in the CMZ, \theObj\ \citep{Tanaka2014}.
{\bf We showed that the cloud had a velocity width of 120 \kmps\ comprising a pair of broad velocity lobes with a velocity width of 60 \kmps\ each, which were anti-correlated with each other in both space and velocity. }
The kinetic energy of the entire system was estimated to be $10^{49}$ ergs, which is comparable to those of the clouds interacting with supernova remnants (SNRs).
We proposed several hypotheses for the origin of the HVCC: cloud--cloud collision, hyper-energetic molecular outflow, a compact expanding shell, and a rotating ring/disk, although the spatial resolution of the telescope ($24''$ = 1 pc) was insufficient to distinguish these possible cases.

{\bf
This paper reports the results of new observations toward \theObj\ performed with the Submillimeter Array (SMA).
We present interferometric images of the cloud in submillimeter lines of HCN, \HCOp, \NNHp, \methanol, and several other hot-core-type molecules probing the dense molecular gas ($n \gtrsim 10^5\ \pcc$) in a wide range of physical and chemical conditions.
The HCN, \HCOp, and \NNHp\ lines are commonly used high density tracers, which are sensitive to different environments; \NNHp\ tends to selectively trace quiescent, cold cores \citep[e.g.][]{Tatematsu2008}, whereas HCN and \HCOp\ abundances are less environmentally dependent and hence they are often useful in detecting shock-compressed gas \citep[e.g.][]{Tanaka2007,Tanaka2014}.
Methanol is one of the most abundant interstellar organic molecules with enhanced abundance in star-forming cores, though other enhancement mechanisms such as cosmic-ray-induced photo-desorption \citep{Yusef-Zadeh2013b} and ejection by shock \citep{Requena-Torres2006} are also suggested to be important in the CMZ.
}
With these data, we investigate the structure of the shocked gas in the cloud in detail and thereby examine whether it shows systematic motion such as collimated outflow, expansion, and rotation, or its large velocity dispersion is caused by random turbulent motion.
We also report the unexpected discovery of compact clumps toward the boundary between the two velocity components of the cloud, which may indicate an early phase of star formation activity under the highly turbulent environment.
In this paper, we adopt 8.3 kpc for the distance to the Galactic center \citep{Gillessen2009}.

\section{OBSERVATIONS}

\subsection{SMA Observations}
The observations were performed on May 12th, 2013, by using the Submillimeter Array (SMA) in the sub-compact configuration providing baseline lengths ranging from 9.5 m to 25 m.
We conducted a hexagonal 7-point Nyquist-sampled mosaic to cover the $52''$ radius region centered at $\left(\alpha_{2000}, \delta_{2000}\right) = (\mathrm{17^h45^m08^s.0}, \mathrm{-29^\circ13'44''.8})$ or $\left(\gl, \gb\right) = \left(-0^\circ.3053, -0^\circ.0622\right)$ in the Galactic coordinates.
The 230 GHz receivers were tuned to observe frequency ranges from 264.77 GHz to 268.75 GHz (LSB) and from 276.77 GHz to 280.75 GHz (USB) simultaneously.
The correlator configuration was chosen to provide  4 GHz frequency coverage in each sideband and 812.5 kHz spectral resolution.
The HCN \JJ{3}{2}, \HCOp\ \JJ{3}{2}, and \methanol\ $J_K$=\meta, \metb, and \metc\ lines were observed in the LSB, and the \NNHp\ \JJ{3}{2}, \CtS\ \JJ{6}{5}, \OCS\ \JJ{23}{22}, o-\HHCS\ $J_{K_{\rm a},K_{\rm c}}=8_{1,7}$--$7_{1,6}$, and \methanol\ $J_K$=\metd\ lines were in the USB.
We list the target lines in Table \ref{TABLE1}, along with their rest frequencies and  upper state energies.

We observed Neptune, 3C279, and nrao530 for the flux, bandpass, and gain calibration measurements, respectively.
We employed the CASA package developed for the NRAO for flagging bad data, applying calibrations, and creating images.
We applied Briggs weighting for the imaging, which provided a $8''.2\times5''.2$ synthesized beam for HCN \JJ{3}{2}.
The beam position angle is $-0^\circ.5$ in the equatorial coordinates or $-59^\circ.1$ in the Galactic coordinates.
Phase-only self-calibration was applied to the quasi-continuum data in each sideband, the calibration table of which was transferred to the line data.
The continuum image was constructed by integrating the emissions of the line-free channels in the total 8 GHz bandwidth.
The total on-source integration time was 25 min per pointing, and the resultant r.m.s. noise level of the final maps is 0.22 \Jypb\ per velocity channel for the USB, 0.27 \Jypb\ for the LSB, and 3.9 \mJypb\ for the continuum data.
Correction for the primary beam was not applied.
The maps were originally made in the equatorial coordinate system, and subsequently we converted them into the Galactic coordinate system for convenience of comparison with the single-dish HCN \JJ{4}{3}\ data obtained with the ASTE 10-m telescope \citep{Tanaka2014}.

\begin{deluxetable}{lcccc}
\tablecaption{Molecular Lines Observed with the {\bf SMA}}
\input{table1.tex}\label{TABLE1}
\end{deluxetable}

\subsection{ASTE Observations}
We also use the published data of HCN $\JJ{4}{3}$ and $\COt\ \JJ{3}{2}$ obtained with the ASTE 10-m telescope \citep{Tanaka2014}.
The maps were obtained with $24''$ spatial resolution and $2\ \kmps$ velocity resolution by employing the On-The-Fly (OTF) scan mode.
The r.m.s. noise levels in the main-beam temperature scale are 0.13 K and 0.21 K for the HCN and \COt\ data, respectively.
Further details of the ASTE data and observations are described in \cite{Tanaka2014}.

\section{RESULTS}
\begin{figure*}[hhh]
\epsscale{1}
\plotone{fig1.eps}
\caption{Maps of the peak flux densities of the observed lines and the continuum flux densities.  The peak flux densities are calculated from spectra binned over 10 velocity channels. The synthesized beam is represented by a filled ellipse on the HCN \JJ{3}{2}\ panel.  } \label{FIG1}
\end{figure*}

\begin{figure*}[hhh]
\epsscale{1}
\plotone{fig2.eps}
\caption{Galactic longitude--velocity diagram of \theObj\ averaged over the full latitude range in HCN \JJ{3}{2}\ and \NNHp\ \JJ{3}{2}\ obtained with the SMA observations, along with the HCN \JJ{4}{3}\  and \COt\ \JJ{3}{2}\ images obtained with the ASTE observations.  The dark hatched region on the leftmost panel indicates the velocity range affected by the artificial velocity gap in the synthesis observation.} \label{FIG2}
\end{figure*}

\subsection{Overall Structure: Central Clump and Extended Turbulent Component}
Figure \ref{FIG1} shows the peak flux densities of the observed lines and continuum flux density, where the peak flux densities were calculated from spectra binned over 10 velocity channels to improve S/N ratios.
Two spatial components can be recognized in the maps.
One is the bright compact clump toward the field center, which is commonly seen in all the observed lines and  the continuum but more clearly in the maps of the optically thinner group (i.e., the continuum and the lines other than HCN and \HCOp).
This central clump is point-source-like in the methanol, \OCS, \CtS, and o-\HHCS\ maps, whereas its \NNHp\ and continuum images have sizes significantly larger than the beam size.
The other component is the clumpy, spatially extended component within a radius of approximately $30''$ around the central clump.
This extended component is dominant in the HCN and \HCOp\ maps and is recognizable in the maps of \NNHp\ and \methanol\ \metb\ and \metd\ as well as the continuum.
The mass distribution is better represented by the optically thin group, indicating that the major fraction of the cloud mass is confined in the central clump.

The contrast between the central clump and the extended component is more striking in Figure \ref{FIG2}, which shows the position--velocity ({\it P}--{\it V}) diagrams along the Galactic latitude axis for the SMA data of the HCN and \NNHp\ lines averaged over the full latitude range.
The extended component in the HCN map shows a highly turbulent velocity structure with emission spanning in a \vlsr\ range of 145 \kmps\ from $-35\ \kmps$ to $+110\ \kmps$, which is wider than that previously measured with our single-dish observations.
In contrast, the central clump in the \NNHp\ image is strictly limited to a narrow velocity range from $-10\ \kmps$ to $+10\ \kmps$, apparently decoupled from the outer highly turbulent flow.
The HCN image has a peak toward the central clump at a velocity slightly blue-shifted by $5\ \kmps$ presumably because of self-absorption.
We also show the single-dish HCN \JJ{4}{3}\  and \COt\ \JJ{3}{2}\ data in Figure \ref{FIG2}, in which only the extended component is visible; they do not have a narrow peak at the velocity corresponding to the central clump.

The emission gap of 15 \kmps\ width at $\vlsr\sim+15\ \kmps$ seen in the SMA HCN \JJ{3}{2}\ data in Figure \ref{FIG2} is likely to be an artifact {\bf resulting from the limited $uv$ coverage in our observations.}
The single-dish \COt\ map shows that the emission in this velocity range extends beyond the primary beam of the SMA, implying that it is resolved out in the synthesis observation.

\subsection{Double-lobed Structure: Tight Anti-correlation between the Broad Velocity Lobes}

\begin{figure*}[ttt]
\epsscale{1.}
\plotone{fig3.eps}
\caption{Peak flux density/brightness temperature maps for the blue-shifted lobe (leftmost; $\vlsr$ range from $-35\ \kmps$ to $+15 \kmps$), intermediate velocity range (second from  left; from $+15$ \kmps to +40 \kmps), and red-shifted lobe (third from left; from +40 \kmps\ to +110 \kmps).  The top and bottom rows are for the SMA HCN \JJ{3}{2}\ and  ASTE \JJ{4}{3}\ data, respectively.  The rightmost panel of the upper row is a schematic diagram showing the positions of the central ridges in the blue- and red-shifted lobes (shown in blue and red, respectively) and the central clump.  The coverage of the SMA observation is superposed on the HCN \JJ{4}{3}\ maps.  }\label{FIG3}
\end{figure*}

\begin{figure*}[ttt]
\epsscale{1.}
\plotone{fig4.eps}
\caption{Composite color images of the two broad velocity lobes, in which the $3\ \sigma$ emission regions of the blue-shifted and red-shifted lobes are shown in cyan and red, respectively, and overlapping regions are shown in white. The region corresponding to the central ridges is encircled by yellow dashed lines.  The methanol peaks A--H are indicated by cross marks.  }\label{FIG4}
\end{figure*}

\begin{figure}[ttt]
\epsscale{0.7}
\plotone{fig5.eps}
\caption{HCN \JJ{3}{2}\ position--velocity diagrams along the horizontal strips passing thorough northern end ($b = -0^\circ.059$),  midpoint ($-0^\circ.064$), and southern end ($-0^\circ.069$) of the central ridges.  The bridging emission between the two broad velocity lobes are indicated by dashed lines. The artificial velocity gap in the synthesis observation is hatched in gray.}\label{FIG5}
\end{figure}

\begin{figure*}[ttt]
\epsscale{1.}
\plotone{fig6.eps}
\caption{Galactic latitude--\vlsr\ diagrams of HCN $\JJ{3}{2}$ at every $10''$ Galactic longitude, with contours of \methanol\ $J_K=\metd$ overlaid. The contour levels are $(3, 5, 10,$ and $ 20)\times \sigma$ ($\sigma = 0.10$ Jy\,beam$^{-1}$). The HCN and \methanol\ spectra are smoothed with Gaussian kernels of 2 \kmps and 5 \kmps\ FWHM, respectively.  Bright methanol peaks are labeled as A--H.  The hatched regions are for the artificial velocity gap in the synthesis observation. }\label{FIG6}
\end{figure*}

The double-lobed structure detected with the ASTE 10-m telescope observation is also clearly recognizable in the SMA image with the improved resolution.
The {\it P}--{\it V}\ diagram of HCN \JJ{3}{2}\ presented in Figure \ref{FIG2} shows that the two broad velocity lobes are sharply separated in space at $\gl = -0^\circ.306$, with a narrow overlapping \vlsr\ range from +15\ \kmps\ to +35\ \kmps.
Figure \ref{FIG3} shows the peak flux density maps of the HCN \JJ{3}{2}\ for the $\vlsr$ ranges of the blue-shifted lobe (from $-35$ \kmps\ to $+15$ \kmps), the intermediate velocity range (from $+15\ \kmps$ to $+40\ \kmps$), and the red-shifted lobe (from $+40$\ \kmps\ to $+110$\ \kmps), along with the single-dish HCN $\JJ{4}{3}$ maps for the same velocity ranges.
The SMA images reveal that the two broad velocity lobes have a ridge-like shape; each broad velocity lobe has a vertical structure near the field center, as schematically shown in the upper rightmost panel.
Hereafter we refer to this pair of parallel ridges as the central ridges.
The emissions from the red-shifted lobe primarily arise from the central ridge part.
The blue-shifted lobe also shows bright emissions in the eastern region behind the central ridge, making the entire lobe appear inverse-`c' shaped.
The central clump is located toward the mid-point of the blue-shifted central ridge.
The emissions from the intermediate velocity range ($-15\ \kmps$ to $+40\ \kmps$) are mostly extensions from the two broad velocity lobes, and no notable spatial structures intrinsic to this velocity range are detected.

Figure \ref{FIG4} shows composite color images constructed from the two broad velocity lobes, where the 3 $\sigma$ emission regions of the blue- and red-shifted lobes are shown in cyan and red, respectively.
As reported in \cite{Tanaka2014}, the two velocity lobes in the single-dish image show a good spatial anti-correlation, with a narrow overlapping region of an about half the beam size.
Now we recognize that the anti-correlation is much tighter in the interferometric images;
the central ridges correspond exactly to the overlapping region in the single-dish image, but they have almost no spatial gaps and only few overlaps between each other.
Thus the two broad velocity lobes appear to contact each other at a well-defined interface on the plane of the sky.
A natural explanation for this remarkable structure is that the two components with different velocities physically interact with each other, that is, they collide.
Meanwhile, our results do not completely exclude other interpretations, as the paired ridges also seem to compose one elongated ring.
We will discuss this issue further in later sections (\ref{DISCUSSION1}, \ref{DISCUSSION2}).

The emissions of the central ridges partly mix in the intermediate velocity range.
Figure \ref{FIG5} shows the {\it P}--{\it V}\ diagrams of the SMA HCN \JJ{3}{2}\ data along horizontal paths across the northern end ($\gb = -0^\circ.59$),  midpoint ($\gb = -0^\circ.64$), and  southern end ($\gb = -0^\circ.69$) of the ridges.
We find several features bridging the velocity gap between the central ridges along these paths.
Along the central strip, the two velocity components are smoothly connected by emission with a velocity gradient in a \vlsr\ range from $-30$\ \kmps\ to +60\ \kmps, except for the artificial emission gap noted in the previous subsection.
A bridging feature is also detected along the northern strip in a narrower \vlsr\ range from +20\ \kmps\ to +40\ \kmps.
The southern strip lacks detectable emission in the intermediate velocity range, although it is possibly because of the missing flux.

\subsection{Broad HCN Emission}
Figure \ref{FIG6} shows the HCN \JJ{3}{2}\ {\it P}--{\it V}\ diagrams along the Galactic latitude at every $10''$ Galactic longitude, with contours of \methanol\ \metd\ emission overlaid, where the HCN and \methanol\ spectra are smoothed with Gaussian kernels of 2\ \kmps\ and 5\ \kmps\ FWHM, respectively.
The broad velocity lobes are resolved into a number of smaller broad emissions.
The red-shifted lobe ($\vlsr \gtrsim +40\ \kmps$) is found to comprise at least 6 broad features with about $10''$ sizes and velocity widths of 40 -- 50 \kmps\ in FWZI, the systemic velocities of which are distributed in a $\vlsr$ range from $+35\ \kmps$ to $+90\ \kmps$ without apparent order.
The blue-shifted lobe ($\vlsr \lesssim +15\ \kmps$) does not seem to have prominent broad features but rather seems to be an ensemble of relatively narrow clumps, although this is at least partly because of the artificial emission gap at $\vlsr \sim +15\ \kmps$; any broad features in this velocity range would be unrecognizable as they would be divided by this artificial gap.
The narrow emissions in the $\vlsr$ range from $-30\ \kmps$ to $-20\ \kmps$ could be the low-velocity ends of such obscured broad features.

The broad emission features are predominantly associated with the central ridges mentioned in the previous subsection, which correspond to the Galactic longitude range from $-0^\circ.303$ to $-0^\circ.308$ in Figure \ref{FIG6}.
They are rather randomly distributed in the position-velocity space, in which we cannot detect definitive signs of systematic motion over the entire clump, such as coherent expansion, rotation, and linear collimated flow.

We label 8 bright methanol peaks as A--H in Figure \ref{FIG6}, the positions of which on the $\gl$-$\gb$ plane are also shown in Figure \ref{FIG4}.
Peak A is the methanol peak in the central clump.
All of the methanol peaks have velocity widths of $10$--$20\ \kmps$, which are narrower than those of the HCN emissions.
They are primarily associated with the broad HCN features in the central ridges, except for peak B, which is located well outside the ridges, and peak H, which is located inside the red-shifted ridge but has an inconsistent blue-shifted velocity.
{\bf
We list the positions of the methanol peaks in Table \ref{TABLE2}, along with their center LSR velocities and FWHM velocity widths determined by Gaussian fitting of the \metb\ spectra.
}

\begin{deluxetable}{lrrrrl}
\tablecaption{Methanol Peaks}
\input{table2.tex}\label{TABLE2}
\end{deluxetable}

\subsection{Central Clump}
\begin{figure}[ttt]
\epsscale{0.6}
\plotone{fig7.eps}
\caption{(a) SMA images of the central clump in the continuum flux density (left) and the $\NNHp\ \JJ{3}{2}$ velocity-integrated flux density (right).  The integration range is from $-10\ \kmps$ to $+20\ \kmps$. The overlaid contours are the \methanol\ $J_K=\metc$ flux integrated over the same velocity range, drawn at every 1 $\sigma$ from 5 $\sigma$ ($\sigma = 1.5\ {\mathrm{Jy\,beam^{-1}}}\ \kmps$). The boundary between the central ridges is schematically drawn with a dashed line on each panel. (b) Spectral energy distribution of the central clump in the far-infrared wavelengths, constructed from 70 -- 500 $\micron$ flux density from the {\it Herschel} data archive. The best-fit gray-body curve (solid line) and 1-$\sigma$ deviation (hatched region) are overlaid. }\label{FIG7}
\end{figure}

Figure \ref{FIG7}a shows the SMA images of the central clump in the continuum, and the $\NNHp\ \JJ{3}{2}$\ and \methanol\ \metc\ flux densities integrated over a velocity range from $-10\ \kmps$ to $+20\ \kmps$.
{\bf Table \ref{TABLE3} summarizes the properties of the central clump.}
The clump has approximately the same elliptic shape in the continuum and in the \NNHp\ maps; they are elongated in the northeast--southwest direction with FWHM sizes of $13''\times8''$.
The point source-like methanol \metc\ emission is offset from the center position of the clump toward the south-western edge, i.e., toward the boundary between the two velocity components.

We estimate the dust luminosity mass of the central clump by referring to the {\it Herschel} archival data.
First, we determine the dust temperature ($\Td$) by analyzing the spectral energy distribution (SED) constructed from the 70--500\ \micron\ flux densities taken from the {\it Herschel} data archive.
Figure \ref{FIG7}b shows the SED for the central $40''$ square region, where contributions from extended emission unassociated with the cloud are subtracted by taking the background position at $\pm60''$ offset from the cloud center in the Galactic longitude and latitude.
The error bars include the calibration errors in the {\it Herschel} data and uncertainties of the background levels estimated using the standard deviations among the flux densities toward the four reference positions.
The SED is consistently fitted by a single-component gray-body model with a dust temperature ($\Td$) of 18 K and the dust emissivity index ($\beta$) assumed to be 2.0.
Although a simultaneous SED fitting of $\Td$ and $\beta$ suggests a higher $\beta$ value of 2.8, we fix $\beta$ at the conservative value of 2.0.
This result is consistent with former observations \citep[e.g.][]{Pierce-Price2000,Molinari2011} indicating that the dust temperatures are uniformly $\sim20$ K throughout the CMZ.
No significant excess in short wavelengths is detected.
The mass of the central clump is estimated to be $5.8\times10^2 \Msol$ from this dust temperature and the 1.1 mm continuum luminosity (0.38 Jy) measured for the entire clump with our SMA data.
We obtain the mean density $n_0 = 5\times10^5\ \pcc$ from the mass and  size of the clump by roughly assuming the volume to be $\frac{4}{3}\pi r^3$.
This is consistent with the density estimate obtained from the excitation analysis of the HCN intensities \citep{Tanaka2014}.

We estimate the viral mass (\Mvt) of the central clump by using the formula $\Mvt/\Msol = 210\,(r/{\mathrm pc})\cdot(\dv/\kmps)^2$ used in \cite{Miyazaki2000} for the CS clumps in the CMZ.
The radius $r$ is estimated as $\frac{1}{2}D\sqrt{\theta_{\mathrm{maj}}\cdot \theta_{\mathrm{min}}} = 0.15\ \pc$, where $D=8.3$ {\bf kpc} is the distance to the source and $\theta_{\mathrm{maj,\ min}} = 10''.2,\ 6''.6$ are the major and minor axis lengths corrected for the instrumental broadening due to the finite beam size, respectively.
The FWHM velocity width $\dv$ is measured to be $12.4\ \kmps$ from the averaged \NNHp\ spectrum, after correction for broadening due to unresolved hyperfine structures.
These values yield  $\Mvt = 4.8\times10^3\ \Msol$.
The virial parameter $\ifmmode{\alpha_{\rm vir}}\else{$\alpha_{\rm vir}$}\fi \equiv \Mvt$/$M$ is $8.3$, which is only slightly smaller than the typical value for the CMZ clouds, $\sim 10$, estimated from the CS \JJ{1}{0}\ observations by \cite{Miyazaki2000}.
By considering the rather large uncertainties in dust and gas properties, we conclude that the central clump is not significantly different from the typical CMZ clouds in \ifmmode{\alpha_{\rm vir}}\else{$\alpha_{\rm vir}$}\fi.

\begin{deluxetable}{lc}
\tablecaption{Properties of the Central Clump and the Methanol Peaks}
\input{table3.tex}\label{TABLE3}
\end{deluxetable}

\subsection{Methanol Peaks}
\begin{deluxetable}{lrrrrrrrrrr}
\tablecaption{Line Fluxes toward Methanol Peaks in Jy \kmps}
\input{table4.tex}\label{TABLE4}
\end{deluxetable}

\begin{figure}[ttt]
\epsscale{0.7}
\plotone{fig8.eps}
\caption{(a) Methanol rotation diagram toward peak A, with the best-fit curve of a single-temperature LTE analysis overlaid (left), and the results of non-LTE excitation analysis, in which the parameter ranges calculated from the observed flux density ratios of $J_K=\meta$ and \metc\ to \metb\ are hatched in red and gray, respectively (right).  In the latter analysis, we assume $10\%$ relative error for each flux density in addition to the spectral noise levels.  (b) Same as (a) but for the stacked data for the methanol peaks B--H.}\label{FIG8}
\end{figure}

{\bf
Table \ref{TABLE4} lists the fluxes of the lines detected toward the methanol peaks A--H.
Toward the methanol peaks outside the central clump, i.e., peaks B--H, only  two methanol transitions, \metb\ and \metd, and the \NNHp\ line are detected above the 3-$\sigma$ levels.
We use a stacking analysis to estimate the fluxes of the undetected lines toward peaks B--H; their spectra are co-added after correction for the difference in the central velocities.
All the lines except \CtS\ \JJ{5}{4}\ are detected above the 3-$\sigma$ levels in the stacked spectra, the fluxes of which are listed in the bottom line of Table \ref{TABLE4}.
}

The left column of Figure \ref{FIG8} shows methanol rotation diagrams constructed from the spectra toward the methanol peak A and the spectra stacked for peaks B--H, in which the upper state column densities per unit velocity (${\rm d}N_{\rm u}/{\rm d}v$) divided by the statistic weights ($g_{\rm u}$) are plotted against their excitation energies for the four methanol transitions.
The ${\rm d}N_{\rm u}/{\rm d}v$ values are calculated from averaged flux densities over the three central velocity channels around the \metb\ peaks by assuming the optically thin condition.
For the central clump, the flux densities of three out of the four transitions are successfully fitted by a single-temperature local thermodynamical equilibrium (LTE) model with a rotation temperature ($T_{\rm rot}$) of 28 K, but the remaining \metd\ transition has an inconsistently high value possibly because the \metd\ transition is masing.
\cite{Yanagida2014}\ detected {\bf class-I maser emissions} of this methanol line that are associated with molecular outflow sources in the infrared dark cloud G34.43+00.24 MM3.
{\bf Peak A also coincides with a source in the list of 36 GHz class-I methanol maser candidates by \cite{Yusef-Zadeh2013b}.
Therefore, we exclude the \metd\ transition in our data from the excitation analysis, although it is yet to be confirmed whether the transition is actually masing because its spectral profile is similar to those of thermal lines and lacks sharp peaks typical for maser profiles.}
For the stacked data of the methanol peaks B--H, a single temperature LTE fit is less successful, and the uncertainty in the rotational temperature is accordingly larger.
The best fit $T_{\rm rot}$ value is again 28 K.

We perform a non-LTE excitation analysis to estimate the physical conditions of the methanol peaks by assuming the optically thin condition.
The rate coefficients for the radiative and collisional transitions are taken from the Leiden atomic and molecular database \citep{Schoier2005}.
The right column of Figure \ref{FIG8} shows the ranges of gas kinetic temperature (\Tkin) and molecular hydrogen density (\nHH) that reproduce $\pm 1\ \sigma$ values around the measured flux density ratios among the \meta, \metb, and \metc\ transitions.
In this analysis, we conservatively assume 10\%\ relative errors in the flux densities (i.e. 14\% in the ratios) in addition to the spectral noises.
In the result for peak A, the \meta/\metb\ and \metc/\metb\ ratios give a consistent parameter range, showing that $\nHH \sim 10^{6.5\mbox{--}7.5}\ \pcc$ with a reasonable assumption for the gas temperature, $40 < \Tkin < 100\ \kelvin$ \citep{Martin2004,Nagai2007}.
For the stacked data for the methanol peaks B--H, the parameter ranges calculated from the two flux density ratios do not overlap.
If we adopt the result for the \metc/\metb\ ratio, which has a higher S/N ratio than the other ratio, we obtain a \nHH\ range similar to that deduced for peak A.
{\bf The parameters derived in this subsection are listed in Table \ref{TABLE3}.}

\section{DISCUSSION}
\subsection{Kinematics of CO$-0.30-0.07$}
In our previous paper \citep{Tanaka2014}, we presented four hypotheses for the origin of the broad velocity emission of \theObj: cloud--cloud collision, expansion driven by blast wave, molecular outflow, and rotation around an invisible massive object.
We discuss these hypotheses in this subsection.

\subsubsection{Cloud--Cloud Collision}\label{DISCUSSION1}
\begin{figure}[ttt]
\epsscale{0.5}
\plotone{fig9.eps}
\caption{(a) Position--\vlsr\ diagram of the ASTE \COt\ \JJ{3}{2}\ data along the path defined in panel b, with contours drawn at every 2 $\sigma$ starting from 3 $\sigma$ ($\sigma = 0.11\ \kelvin$).  The velocity ranges of the +15-\kmps\ and +55-\kmps\ clouds are indicated.  (b) Composite color image constructed from the \COt\ \JJ{3}{2}\ integrated intensities of the +55-\kmps\ and +15-\kmps\ clouds (red and blue color channels, respectively).  Contours of the peak HCN \JJ{3}{2}\ flux densities of the red- and blue-shifted lobes in the SMA data are overlaid and shown in red and blue, respectively. The contours are drawn at 3 $\sigma$\ intervals starting from 7 $\sigma$ ($\sigma = 0.28\ {\mathrm{Jy\,beam^{-1}}}$).}\label{FIG9}
\end{figure}
With the interferometric HCN \JJ{3}{2}\ image taken with the SMA, we found remarkably tight anti-correlation between the two broad velocity lobes comprising \theObj, which is much tighter than that previously found with single-dish ASTE observations;
the characteristic broad velocity emissions are predominantly confined in the central ridges running through the cloud center, and the individual ridges in the two velocity components are tightly anti-correlated with each other on the plane of the sky.
Thus the entire cloud appears to be sharply divided into the two velocity components by the linear boundary defined by the central ridges.

We can give a natural explanation for this structure by assuming that the cloud is a pair of colliding clumps.
In the numerical model of colliding clouds by \cite{Gilden1984}, planar compressed layers appear behind the shock fronts propagating away from the collision interface and into the individual clouds.
The central ridges of \theObj, which run along the interface between the two velocity components, are consistent with this model.
The turbulent velocity in the post-shock region is expected to be enhanced up to the shock velocity \citep{Inoue2013b}.
For \theObj, the minimum value of the collision velocity \vcol\ is roughly estimated to be $20\ \kmps$, i.e., half of the  \vlsr\ difference between the two velocity components, although the edge-on geometry of the collision interface may indicate that the tangential collision velocity is faster than the line-of-sight velocity.
The velocity dispersion of 18\ \kmps\ inside the red-shifted lobe is consistent with this collision velocity within the uncertainty in the tangential velocity.

We can identify a spatially extended part of each of the colliding pair in the single-dish \COt\ \JJ{3}{2}\ map.
Figure \ref{FIG9}a is the {\it P}--{\it V}\ diagram of the \COt\ \JJ{3}{2}\ data along the diagonal path across the cloud indicated in Figure \ref{FIG9}b.
The figure shows multiple components in the velocity range from $-50\ \kmps$ to $+90\ \kmps$ in addition to the broad emissions of \theObj.
The blue-shifted lobe of \theObj\ is obviously associated with the +15-\kmps\ cloud, the most intense and most widespread component in the map.
The red-shifted lobe also accompanies a spatially extended, narrow component at $\vlsr\sim+55\ \kmps$.
This +55-\kmps\ cloud is elongated from the south-western direction and is truncated at the position where it intersects the red-shifted lobe.
Figure \ref{FIG9}b shows a composite color image constructed from the single-dish \COt\ data, in which the +15- and +55-\kmps\ clouds are shown in blue and red, respectively.
The figure illustrates that the broad velocity lobes observed in the SMA data (indicated by the contours in the figure) are well correlated with the boundary between the +15- and +55-\kmps\ clouds.
This configuration, i.e., compact broad emissions at the contact points of two clouds with narrower line widths, is typical for a cloud--cloud collision system \citep[e.g.][]{Duarte-Cabral2011}.

A major argument against the cloud--cloud collision scenario is that a part of the shocked region is actually extended well behind the interface between the two clouds in our data; the blue-shifted lobe also has bright emissions in the eastern part of the cloud, where it lacks a red-shifted counterpart (Figure \ref{FIG3}).
In order to explain this feature, we have to adopt additional, ad hoc assumptions such as that the red-shifted counterpart is somehow invisible or has already dissipated or that there is another source of turbulence in the eastern side of the +15-\kmps\ cloud.

\subsubsection{Expanding Molecular Ring Model}\label{DISCUSSION2}
\begin{figure*}[ttt]
\epsscale{1.}
\plotone{fig10.eps}
\caption{a) The first moment map of the SMA HCN \JJ{3}{2}\ data, with the colors and brightness representing the first velocity moment and peak flux density, respectively.  (b) Angular variation of the first moment along the ellipse defined in panel a. The definition of the position angle $\theta$ is also given in panel a.  The overlaid curve is for an expanding-ring model with an expansion velocity $\vexp$ of 45\ \kmps and inclination angle of $62^\circ.5$.  (c) Same as (b) but with model curves for rotating-ring models with various assumptions for the inclination angle $i$.  The maximum line-of-sight velocity is fixed at 80 \kmps.  The attractor loci are assumed to be the northern and southern focal points in models-1 (left) and -2 (right), respectively.}\label{FIG10}
\end{figure*}
An expanding ring driven by a blast wave is also a good model for the cloud kinematics, if we ignore the spatial anti-correlation between the central ridges by regarding it as coincidental.
In the ring model, the two ridges are assumed to be portions of an ellipse elongated in the Galactic north--south direction, as indicated in Figure \ref{FIG10}a.
The figure also shows the first velocity moment map of the SMA HCN \JJ{3}{2}\ data.
The cloud has an overall velocity gradient across the major axis of the ring, which is interpreted as expansion rather than rotation by adopting the natural assumption that the ring is nearly circular in the three-dimensional space with a large inclination from the plane of the sky.
The other possible kinematics, that is, a model of a highly elliptical rotating ring inclined around the minor axis, is discussed in the next sub-subsection (\ref{DISCUSSION3}).

Figure \ref{FIG10}b\ shows the angular variation of the first moment of the ring defined in Figure \ref{FIG10}a, along with the model curve for an expanding ring with an inclination of $62^\circ.5$ and expansion velocity of $45\ \kmps$.
Although we have failed to detect clear signs of coherent expansion motion in the {\it P}--{\it V}\ diagrams (Figures \ref{FIG2} and \ref{FIG6}), the first moment variation in Figure \ref{FIG10} is successfully fitted by the expansion model; both the model and observation show steep gradients at the tangential points ($\theta\sim0^\circ,\ 180^\circ$) and rather flat curves in the other parts.
The failure in the detection of coherent expansion in the three-dimensional {\it P}--{\it V}\ images could be explained as being the result of disturbance caused by interaction with non-uniformly distributed outer media; such a situation would be expected for an expanding ring driven by explosion in the vicinity of a dense molecular cloud.

An advantage of the expanding-ring model over the collision model is that it can easily explain the feature unassociated with the central ridges without additional assumptions because an isotropic explosion can create shocked regions also outside the expanding ring.
A problem with the expansion model is that the region inside the assumed ring is actually not an emission cavity; it shows low-level emissions smoothly bridging the velocity gap between the central ridges, as shown in Figure \ref{FIG5}.
The central ridges are most smoothly bridged at their midpoints by a horizontal structure, making the ring appear to be shaped like the symbol $\Theta$.
The expanding-ring model cannot provide a simple explanation for the horizontal bar structure.
In addition, the absence of visible energy sources capable of driving the fast expansion motion, the kinetic energy of which is estimated to be $4\times10^{49}\ \ergs$ from the total mass of \theObj\ \citep[$10^3\ \Msol$;][]{Tanaka2014} and the expansion velocity (45 $\kmps$), remains as a major problem; {\bf the cloud is not associated with any sources in the published catalogs for radio \citep{Nord2004,Lazio2008} or X-ray \citep{Muno2006} sources.}
We also note that the first moment variation displayed in Figure \ref{FIG10}b\ is insufficient to distinguish between the collision model and expanding-ring model because the observed pattern is expected for any cases involving two distinct velocity components of similar sizes along the path.

\subsubsection{Other Scenarios}\label{DISCUSSION3}
The other two models in \cite{Tanaka2014}, namely the rotating-ring/disk and the hyper-energetic outflow scenarios, do not fit the observation.
If we assume that the central ridges represent an elliptic Keplarian orbit around a compact massive object, the large eccentricity implies that the attractor is very close to either end of the major axis and that very steep velocity gradients should appear at the pericenter passage as a result.
In Figure \ref{FIG10}c we show two rotation models corresponding to the two possible attractor loci (i.e., the northern and southern focal points) with various inclinations and a fixed maximum line-of-sight velocity of 80 \kmps.
Neither model reproduces the observed line of sight velocities, especially those near the pericenter passage.
The models with low inclinations, which show milder velocity variation near the pericenter, may seem to fit the observation better, but they require unrealistically large attractor masses: $1\times10^6\ \Msol$ and $1\times10^7\ \Msol$ for inclinations of $30^\circ$ and $10^\circ$, respectively.

The bipolar-outflow model is also unsuccessful; the broad emissions are not linearly aligned  as expected from the outflow model.

\subsubsection{The Origin of the Broad Emissions}
We have shown that the cloud--cloud collision model gives the most reasonable explanation for the cloud kinematics and the absence of visible energy sources with fewer assumption than the other three models.
We can safely rule out the rotating-ring and  bipolar-outflow models with our observations.
The expanding-ring model cannot be completely excluded, because it reproduces the observed velocity structure of the cloud very well for a limited spatial range.
Further investigation of the shock structure with a better resolution will help to determine whether the shocked gas represents a collision interface or is shaped as an elongated expanding ring.

\subsection{Implications of the Shock-Triggered Star Formation}
Our SMA observations toward \theObj\ have revealed a remarkable structure quite different from that known from previous observations: a compact, quiescent clump with bright \NNHp\ and continuum emissions co-exists with the highly turbulent gas traced by the HCN and \HCOp\ lines.
We also detected at least 8 point source-like, bright methanol peaks, including one in the central clump.
The densities of the methanol peaks are deduced to be $\sim 10^{6.5\mbox{--}7.5}\ \pcc$ from the excitation analysis with the multi-transition methanol data.
The high density, compactness in size ($\lesssim 0.1\ \pc$ in radius), and bright methanol emissions suggest their similarity to typical star-forming cores.
Hence, we consider that \theObj\ may provide an ideal test case for star formation in the CMZ, where stars generally form under highly turbulent environments relative to the Galactic disk region \citep{Kruijssen2014,Rathborne2014}.

The central clump and all of the methanol peaks are associated with broad HCN emissions, especially those aligned along the boundary between the two velocity components (Figure \ref{FIG4}).
This suggests that they are density enhancements created via compression by the shock formed at the boundary, irrespective of whether the origin of the shock is cloud--cloud collision or blast-wave impact.
This assumption is corroborated by the widths of the methanol lines; they are  approximately 2--3 times that expected from their sizes and the size--linewidth relationship for the CMZ \citep{Miyazaki2000, Oka2001a}.
The theory of turbulence-regulated star formation \citep{MacLow2004,Krumholz2005,Padoan2011} suggests that the density enhancements in turbulent clouds start collapsing once they become self-gravitating and eventually form stars.
\cite{Inoue2013a}\ show that  high turbulent pressure and enhanced magnetic field strength in cloud--cloud collision systems set a preferable environment for the formation of massive stars.
We may expect such a triggered star formation process in \theObj.

As indicated by the high \ifmmode{\alpha_{\rm vir}}\else{$\alpha_{\rm vir}$}\fi\ of $\sim 10$, the entire central clump is not self-gravitating but likely confined by external ram pressure.
It is unclear whether the central clump and methanol peaks have any self-gravitating substructures capable of forming stars.
Here we investigate whether the methanol peak A in the central clump is sufficiently dense to become self-gravitating, according to the modeling in \cite{Federrath2012}.
The critical density \ncrit\ is given by
\begin{eqnarray}
n_{\rm crit}/n_0 &\sim& A\cdot\alpha_{\rm vir}\cdot\mathcal{M}^2\cdot\left(1+\beta^{-1}\right)^{-1},  \label{EQ1}
\end{eqnarray}
where $n_0$ and $\mathcal{M}$ are the mean density of the cloud and r.m.s. sonic Mach number of the turbulence, respectively, and $A$ is a constant close to unity.
The value $\beta \equiv 2c_{\rm s}^2/c_{\rm A}^2$ is the thermal-to-magnetic pressure ratio, where $c_{\rm s}$ and $c_{\rm A}$ are sound speed and Alfv\'en velocity, respectively.
If the magnetic field is negligible ($\beta\rightarrow\infty$), the critical density is $8\times10^8\ \pcc$ for the central clump when \Tkin = 50 K.
We obtain a lower critical density of $\sim 2\times10^7\ \pcc$ by assuming that $c_{\mathrm{A}} = 3\ \kmps$ from the typical values of the density \citep[$\nHH = 10^{3.5}\ \pcc$; ][]{Nagai2007} and magnetic field strength \citep[$B\sim0.1$ mG;][and references therein]{Ferriere2009} in the CMZ clouds and that the magnetic field is frozen-in to the gas.
The latter value is comparable to the density deduced for peak A, implying that peak A is possibly dense enough to be self-gravitating, although we will need spatially resolved observations toward the methanol peaks in order to make a more conclusive evaluation.
{\bf
Here, we note that the strong tidal field in the CMZ, which is not taken into account in Equation (\ref{EQ1}), does not significantly change the above discussion.
The critical density for self-gravity to overcome the tidal shear is approximately $10^4\ \pcc$ at a Galactocentric radius of 100 pc \citep{Yusef-Zadeh2007}, indicating that the tidal shear is negligible in the density range considered.
}

It may seem that stars are already forming in the methanol peaks in \theObj\ because of the richness of the molecular species detected toward them; bright methanol emission is a major indicator of massive star formation, and \OCS\ and \HHCS\ are also {\bf classified as} hot-core-type molecules \citep{Immer2014a}.
{\bf
However, we refrain from identifying the methanol peaks as hot cores because the hot-core-like chemistry is not limited to star-forming regions in the CMZ; the hot core chemistry without hot cores \citep{Requena-Torres2006} is rather widespread throughout the region, where the molecules formed on the grain surfaces are efficiently evaporated into the gas phase by cosmic-rays and/or shocks in addition to heating by young massive stars \citep{Requena-Torres2006,Menten2008,Yusef-Zadeh2013b}.}
We estimate the fractional methanol abundance to molecular hydrogen toward peak A to be $2\times10^{-7}$ on the basis of the methanol and continuum flux densities by assuming an ortho/para ratio of unity and the LTE condition with a $\Trot$ of 28 K.
{\bf
This high abundance is typical for hot cores but is also well within the range of the abundances measured toward non-star-forming clouds in the CMZ, suggesting that the high methanol abundance toward the methanol peaks might simply reflect the typical chemical composition in the CMZ rather than indicate hot-core formation.
The class-I methanol maser candidates in the \metd\ transition could be further evidence for massive star formation, but it is also possible that they are excited directly by the shock impact rather than by outflow from young stellar objects.
In fact, the 36 GHz class-I methanol maser candidates identified in \cite{Yusef-Zadeh2013b} show poor correlation with known star-forming regions.}
Internal heating sources are also undetected in the dust SED of the central core (Figure \ref{FIG7}b).

The collision-induced cluster formation scenario is a popular explanation for the formation of super star clusters (SSCs) in the CMZ \citep{Hasegawa1994,Higuchi2014}.
\theObj\ is a new candidate for the site of triggered star formation at its early stage, although it is evident that the cloud, the mass of which is $\sim 10^3\ \Msol$, is only capable of forming a cluster of at most a few $100\ \Msol$.
We note that the situation of \theObj\ is similar to that of G0.253+0.016, or the ``brick'', the infrared dark cloud in the CMZ often referred to as a progenitor of a SSC similar to the Arches and the Quintuplet \citep{Longmore2012a,Higuchi2014,Rathborne2014a}.
\cite{Higuchi2014}\ show sulfur monoxide (SO) cores with large velocity dispersion ($\sigma_v$) aligned along an arc-shaped structure, which they argue is an imprint of past impact by a smaller cloud.
The methanol peaks confined in a thin shocked layer in \theObj\ could be smaller versions of these large-$\sigma_v$ SO cores.

\section{SUMMARY}
By utilizing the SMA, we have performed synthesis mapping toward the HVCC \theObj, a peculiar molecular cloud with an extremely broad velocity width in the CMZ.
We summarize the main results below.
\begin{enumerate}
\item The cloud has two distinctive components: a highly turbulent, spatially extended emission traced by HCN and \HCOp\ and a central clump of 0.15 pc radius with bright \NNHp\ and continuum emissions.  The central clump has a narrow velocity width of $12\ \kmps$ in FWHM, which is in striking contrast to the extremely broad emission of the extended component spanning over a 145 \kmps\ velocity range.
\item The extended component has a pair of parallel vertical ridges running through the center of the cloud.  These central ridges are tightly anti-correlated with each other in both space and velocity, thereby dividing the entire cloud into two components with line-of-sight velocities differing by 40 \kmps.
\item The marked broad emissions of the cloud primarily arise from the central ridges, which are again resolved into a number of smaller broad emission features with widths of 40--50\ \kmps\ in the HCN image. These broad HCN emission features are rather randomly distributed in the position--velocity space without apparent order. No pattern indicating systematic motion such as coherent expansion, rotation, or bipolar outflow is detected.
\item The mass of the central clump is estimated to be $5.8\times10^2$ \Msol\ from the continuum luminosity. The virial parameter \ifmmode{\alpha_{\rm vir}}\else{$\alpha_{\rm vir}$}\fi\ is not significantly different from those of typical CMZ clouds, $\sim10$.
\item At least 8 bright methanol peaks are detected toward the central clump and in the central ridges, accompanying several other hot-core-type molecular lines.  Their methanol rotation temperatures are estimated to be 28 K under the LTE assumption.  Non-LTE analysis for the methanol peak of the central clump shows that the molecular hydrogen density is $10^{6.5\mbox{--}7.5}\ \pcc$ under the assumption that $\Tkin = 40\mbox{--}100\ \kelvin$.
\item \theObj\ is located at a position where two larger clouds at $\vlsr = +15$ and +55 \kmps\ contact each other, and the central ridges with broad emissions are well correlated with the boundary between them.  The tight anti-correlation between the ridges suggest that \theObj\ could be a site of cloud--cloud collision.  Meanwhile, another model in which the central ridges are assumed to be parts of a molecular ring expanding at a velocity of 45\ \kmps\ cannot be excluded, as it explains the angular variation of the line-of-sight velocity well.  The other two models proposed in \cite{Tanaka2014}, namely the bipolar-outflow and the rotating-ring models, do not fit the observations.
\item The central clump and the methanol peaks, which have small radii ($\lesssim 0.1\ \pc$), densities marginally high enough to be self-gravitating, and rich abundances of hot-core-type molecules, are similar to typical star-forming cores in the Galactic disk region.  These objects are predominantly aligned along the central ridges and hence are likely to be features created by shock impact.  We speculate that the cloud is at an early phase of shock-triggered star formation, although conclusive evidence for star formation activities is yet to be obtained.
\end{enumerate}

\acknowledgements
The authors are grateful to an anonymous reviewer for his/her helpful comments.
We also thank the SMA staff for their support during the observations reported here.
The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica.

redpajama_set_name: RedPajamaArXiv


text:
Ereignisse
Auf Anraten des Beamten Liu Yan erweitert der chinesische Kaiser Ling die zivilen und militärischen Befugnisse der Gouverneure, um der zahlreichen Bauernaufstände im Reich Herr zu werden. Diese Maßnahme besiegelt den Zusammenbruch der Zentralmacht im Han-Reich. Der Kaiser ernennt auch die Offiziere Yuan Shao, Cao Cao und Chunyu Qiong zu Obersten der Westgarten-Armee.

Geboren

 4. April: Caracalla, römischer Kaiser († 217)
 um 188: Yu Shao, chinesischer General († 242)

Gestorben
 188/190: Marcus Aurelius Cleander, römischer Prätorianerpräfekt

Weblinks

redpajama_set_name: RedPajamaWikipedia


HIND Unilever closed the week on positive note gaining around 0.50%.
As we have mentioned last week that minor support for the stock lies in the zone of 1075 to 1085. Support for the stock lies in the zone of 1030 to 1040 where Fibonacci levels are lying. If the stock manages to close below these levels then the stock can drift to the levels of 1010 to 1020 where Fibonacci levels are lying. During the week the stock manages to hit a low of 1075 and close the week around the levels of 1098.
Minor support for the stock lies in the zone of 1075 to 1085. Support for the stock lies in the zone of 1030 to 1040 where Fibonacci levels are lying. If the stock manages to close below these levels then the stock can drift to the levels of 1010 to 1020 where Fibonacci levels are lying.
Resistance for the stock lies in the zone of 1120 to 1130. If the stock manages to close above these levels then the stock can move to the levels of 1160 to 1170.


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redpajama_set_name: RedPajamaGithub


text:
Send2Press › Wire › General Editorial › Men's Interest › Famed Air Force One Detailers Join P&S Sales to Prep Hundreds of Vintage Classics at Monterey Car Week
Famed Air Force One Detailers Join P&S Sales to Prep Hundreds of Vintage Classics at Monterey Car Week
Source: P and S Sales | Fri, 07 Aug 2015, 08:00:24 EDT
HAYWARD, Calif., Aug. 7, 2015 (SEND2PRESS NEWSWIRE) — Sixteen members of the elite Air Force One Detailing Team led by Master automotive and aircraft detailer, Renny Doyle of Detailing Success and the Detail Mafia, has partnered with Bob Phillips, president of P&S Sales, an innovative professional detailing product manufacturer and distributor, to be the exclusive detailers and detailing product providers at the 24th Annual Gordon McCall Motorworks Revival Event.
Held on Wednesday, August 12 at Monterey Jet Center in Monterey, proceeds from McCall's "Luxury Lifestyle Bash" support the California Highway Patrol 11-99 Foundation.
Over 3,500 of the most influential automotive collectors, car enthusiasts, celebrities, and automotive professionals in the world attend the posh event every year. Phillips (CD-SV, RT) is also a member of Doyle's Detail Mafia, a select brotherhood of high-end professional detailers who specialize in the restoration, maintenance, and preservation of multi-million-dollar automobiles and aircraft. Many members of the team just returned in July from their decade-long preservation of the original Air Force One presidential jet at Seattle's Museum of Flight. They also travel the U.S. restoring and preserving classic and exotic private collections, museum paragons, and community projects nationwide.
Using exclusively P&S Detailing Products, on Tuesday and Wednesday, August 11-12, the team will begin by prepping an entire fleet of rare and exotic automobiles, private jets, and helicopters. The vehicles and the team's talents will be showcased at McCall's Official Kickoff Gala, Wednesday evening from 5 until 10 p.m. The elegant party marks the start of 2015 Monterey Car Week.
On Thursday, August 13, the Detail Mafia and P&S Sales move out to the Monterey Peninsula where they will prep another fleet of vintage sports cars and creme de la creme luxury cars for Friday's The Quail, A Motorsports Gathering at the Quail Lodge & Golf Club. The event's global reputation made it a finalist in the Motoring Event of the Year category for the 2014 International Historic Motoring Awards. Again, the team's unique paint correction and detailing talents will be as much on display as the cars themselves.
On Saturday, August 15, the team heads over to the Rolex Monterey Motorsports Reunion where they will prep and maintain a selection from hundreds of race cars competing in the world's premier motoring event, and the largest event of Monterey Classic Car Week.
Only Master-level and mentored members of Doyle's Detail Mafia have been selected for the events next week, and the products provided by P&S Sales are among the finest on the market today.
"I wasn't sure you could top detailing the first Air Force One presidential jet in terms of celebrated projects," says Doyle. "But when you consider the exclusivity, the elegance, and the special emphasis on luxury, custom, exotic, and vintage automobiles, motorcycles, and even aircraft at these three events, I am awestruck by being trusted with their perfection."
"P&S detailing products are developed and tested for just this kind of high-end, professional work," says Phillips. "To be invited by Gordon McCall himself to provide the exclusive detailing products for events like these would make my late father, Bill, who founded the company, very proud."
For more information about Detail Mafia, visit:
https://www.facebook.com/autodetailingschool
For more information about P&S Sales, visit:
http://psdetailproducts.com/.
* PHOTO for media: Send2Press.com/wire/images/15-0806-detail-mafia-300dpi.jpg
* Caption: Members of The Detail Mafia with P&S Sale's Bob Phillips (far right).
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Original Story ID: 2015-0807-01 (10414) :: famed-air-force-one-detailers-join-ps-sales-to-prep-hundreds-of-vintage-classics-at-monterey-car-week-2015-0807-01
Original Keywords: Luxury Lifestyle Bash, 24th Annual Gordon McCall Motorworks Revival Event, Rolex Monterey Motorsports Reunion, Bob Phillips P and S Sales Hayward California HAYWARD, Calif.
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redpajama_set_name: RedPajamaCommonCrawl


Discover unspoilt Crete while walking from the north to the south coast through beautiful areas that few tourists get to see. This tour will take you from the fertile green agricultural area of Apokoronas via the Lefka Ora (White Mountains) to the pristine beaches of the astonishing south coast, where you will walk through two of its most beautiful gorges: the Sfakia Gorge and the Aradhena Gorge.
Today a challenging walk in the mountains is planned. You will walk up to 1,300m and admire 2,000m peaks, covered with snow in spring. There are no villages in this area; you may occasionally bump into a shepherd with his goats or sheep. The way back down to Askifou is via a beautiful old path through dense forest. Now and then you will have great views to the Askifou plain. In case you prefer a less strenuous walk, you can take the coastal walking route to Loutro, with the option to go for a swim at the Fresh Water Beach.
Via a steep zig-zag path you climb up to the village Anopolis. From here you walk further onto Ancient Aradhena, located on the edge of the impressive Aradhena Gorge. A spectacular path takes you down into the Aradhena Gorge which you follow until you reach the coast. During the last part of today's walk you will follow a path along the coast back to Loutro. It is possible to make a shorter walk of 4 hrs. today via Livaniana (a tiny village) and then descend via the Aradhena Gorge to the sea. It may be necessary, depending on your departure flight tomorrow, to travel today back to Chora Sfakion by ferry and on to Chania or to Heraklion.
Today you travel back to Chora Sfakion by ferry in the morning and, from there, by public transport or pre-booked transfer to Chania or Heraklion Airport.
Loutro: car free and splendid views on the scenic bay. You stay in Protopapas Rooms in basic but well-maintained en-suite rooms.
Breakfast is included on all days. Products for lunch are available in the local shops; at Askifou the shop is 1.5 km from the accommodation and you may ask for a packed lunch or shop in Imbros during the walk. In the evening you have a wide choice of taverns at all locations, except in Askifou where you can only dine at the hotel itself.
Baggage transfers during all walks are included and your bags will be transferred by your current hotel (or by private transfer) to your next hotel. All belongings must be clearly marked with your name. Ask the accommodation owner where and at what time the bags should be left in the morning. During this trip the luggage transfer from Chora Sfakion to Loutro is done per ferry and the hoteliers take care of luggage transportation to and from the ferries. This is quite common in this part of Crete and completely safe. Please have in mind that luggage is not always handled gently, so pack accordingly. When you travel with public transport or on a ferry you always take your luggage with you.
This holiday is appropriate for experienced walkers and requires a very good level of fitness, sure footedness and a head for heights (read more about difficulty grades).
This trip is available between late March and late October. During summer months it can get too hot for hiking. Best month to visit are either spring time (when nature is at its best) or in the autumn (when sea water is still warm). The flexibility of self-guided holidays means that there are no fixed dates and you can start your trip on any date in the season – so please indicate desired beginning date when booking.


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Decarbonization in Vermont: An RFF Report for the Vermont State Legislature
Marc Hafstead and Wesley Look
Getty Images / Glowimages
In July 2018, the Vermont Joint Fiscal Office hired Resources for the Future (RFF) to compile a report on decarbonization policies for the state. The report documents our research on methods to reduce Vermont's greenhouse gas (GHG) emissions. Specifically, we examine both carbon pricing policies (carbon taxes and cap-and-trade programs) and nonpricing policies (incentives for electric vehicles, weatherization programs, etc.). We detail the level of GHG emissions reductions from these policies and compare this with the climate goals of the State of Vermont.
Trends and Greenhouse Gas Reductions
Emissions in Vermont have been increasing since 2011, and the state is not expected to meet its GHG emissions targets with current policies. For example, Vermont statute mandates that state GHG emissions be 58 percent below 2005 levels by 2028, or 50 percent below 1990 levels. Additionally, Governor Scott has set a target, through the US Climate Alliance (USCA), of reducing emissions to levels that are 26–28 percent below 2005 emissions by 2025. Under current policies, however, Vermont emissions are only projected to be 14 percent below 2005 levels in 2028, shy of both above mentioned targets.
In addition, our analysis suggests that Vermont is unlikely to meet its emissions targets with a carbon-pricing-only strategy, unless the carbon price is substantially higher than the prices modeled ($19–$77 per metric ton of carbon dioxide equivalent in 2025). Vermont has a high share of emissions from transportation and heating fuel use, and both of these sectors are difficult to decarbonize.
Our analysis also suggests that by combining moderate carbon pricing and a set of nonpricing policies recommended by the Governor's Climate Action Commission, emissions could be reduced enough to meet the state's USCA target, though not enough to meet the state's statutory target. Under this combined approach, emissions are projected to be 32–38 percent below 2005 levels in 2025, compared with the target of 26–28 percent.
Economic Impacts of Carbon Pricing
The economic impacts of carbon pricing in Vermont, in terms of state GDP, employment, or overall economic welfare, are expected to be very small. Ignoring the environmental benefits of the policy, we project that the total economic costs of the various carbon pricing policies we studied to be between $7.1 and $61.2 million in 2025 ($20–$100 per person, on average).
When we consider the climate and health benefits, each carbon pricing policy is projected to produce benefits that would exceed its economic costs.
Carbon Pricing Revenue Usage
A carbon pricing policy would generate significant revenue for the state: $74.7–$433.8 million in annual revenue in 2025, depending on the carbon price amount and number of sectors covered.
In choosing how to use this revenue, policymakers will face trade-offs between environmental outcomes, overall economic costs, and the impacts on different types of households. One such use is per household rebates (or lump-sum rebates, sometimes referred to as "carbon dividends"). Per household rebates take the net revenue collected from a carbon pricing policy and return it through equal payments to all Vermont households. According to RFF's modeling analysis, per-household rebates more than offset the costs of increased energy prices for the average low-income household.
Carbon pricing revenue can also be used to reduce taxes on wage income. This would lower the overall cost to Vermont's economy relative to other options considered, but these cuts would not fully offset higher energy prices for low-income households.
Devoting revenue to finance nonpricing policies would reduce GHG emissions further, but would also impose higher costs on Vermonters. This is because revenue that could be used to partially or fully offset the economic impacts on households of carbon pricing would instead be redirected toward funding more policies to reduce GHG emissions.
Given Vermont's current emissions profile, with emissions concentrated in transportation and heating fuels, decarbonizing the economy to meet the state's goals will require new, ambitious policy. Our quantitative evaluation suggests that a carbon pricing–only decarbonization strategy in Vermont is unlikely to produce the level of GHG emissions reductions required to meet the state's climate targets (unless, as mentioned above, the carbon price is set substantially higher than levels considered in this study). Our analysis also demonstrates, however, that the combination of a moderate carbon price with a comprehensive set of nonpricing policies (for example, from providing electric vehicle and energy efficiency incentives, to increasing the stringency of the statewide Renewable Energy Standard) could allow the state to meet some, but not all, of its emissions reduction targets. The economic effects of carbon pricing in Vermont are expected to be small; and under all policies we modeled, the public health and climate benefits outweigh total costs. How the revenue from carbon pricing is recycled has important implications for how the costs are distributed throughout the economy—including how low-income and rural households fare compared to upper income and urban households.
The views expressed in RFF blog posts are those of the authors and should not be attributed to Resources for the Future.
Marc Hafstead
Wesley Look


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Home > About HCSO > News Releases > 2019 > June > 19-262
News Releases are to be used for informational purposes only.
Information provided should not be relied upon for any type of legal action.
Release Number: 19-262
Hillsborough County Sheriff's Office
Public Affairs Office : piocommandcenter@hcso.tampa.fl.us
Arrest Made in Murder
Arrest made in murder of 14-year-old girl in Brandon
Dereck Polanco Rivera is also facing a charge of Throwing a Deadly Missile at, within or into a Vehicle (Felony), in addition to a Felony Second Degree Murder charge.
Previous Release:
Arrested:
Dereck Polanco Rivera
The Hillsborough County Sheriff's Office has made an arrest in the shooting death of a 14-year-old girl in Brandon.
Dereck Polanco Rivera, 16, was arrested Tuesday evening, June 25, at his home at 8603 Postwood Circle in Tampa. Rivera is facing a felony charge of Second Degree Murder. Rivera is a certified gang member with the "TC Boys," a gang based in the Town N Country area. The shooting is not believed to be gang related.
Around 1:30 a.m. on Monday, June 17, deputies with the Hillsborough County Sheriff's Office were called to a Walgreens parking lot located at 128 E Brandon Blvd for a report of a shooting. Deputies located a 14-year-old girl in the back seat of a car with a gunshot wound to the head.
Three others were in the vehicle at the time of the shooting, one adult female driver and two additional juveniles.
After interviewing the three witnesses, deputies learned that the occupants had just left a house party on Rollingwood Lane in Valrico.
A male occupant in the vehicle had a long-standing "beef" with Dereck Rivera, which is why detectives believe Rivera targeted the car the young girl happened to be riding in. It is unclear what caused the conflict between Rivera and the male juvenile.
At the intersection of Kingsway Road and East Clay Avenue in Brandon, about a mile from the Walgreens, Rivera fired multiple shots at the vehicle. One bullet went through the rear window, hitting the 14-year-old victim in the head. The victim was taken to Brandon
hospital, then flown to Tampa General Hospital in critical condition, where she died a day later.
Rivera's booking photo is attached. He was transported to the Juvenile Assessment Center (JAC) Tuesday night. At this time, Rivera is facing a charge of Second Degree Murder. The State Attorney's Office will determine if Rivera will be charged as an adult.
No further information is available at this time.
Sheriff Chad Chronister
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Great post. So true! People refuse to realize how capitalism is supposed to work. Little do they realize that communism has been a dismal failure in every society it's been tried…You never end up with all rich people.


James joins forces with ARIA Award-winning indie-pop songstress, Megan Washington, and the genius of jazz piano, Marian Petrescu, for four monumental performances in our capital cities. With her unique, bold style, Washington makes a rare and stunning return to her jazz roots. The fleet-fingered Petrescu, with his dazzling technique and dynamic interpretation, is eclectic and adventurous, rounding out this trio to near perfection.


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News Tige Boats Adds Phenom Cobe France To Team
Tige Boats Adds Phenom Cobe France To Team
Tige Boats is proud to announce Cobe France as the newest addition to the TeamTige Global Wakeboarding Team. Cobe is making a statement at 14 years old as a WWA Junior Boys World Champion and is in training with wakeboarding legends to accomplish his mission of becoming the future of the sport.
"Cobe has a solid vision: he rides constantly, he trains with the best, and he is determined to claim the future of wakeboarding," stated Daniel Gutierrez, Director of Design and Marketing for Tige Boats. "We are stoked to cultivate one of the most talented up and coming riders in the world."
"I have been training behind Tige's for my whole life and I am so stoked that I am now a part of their team," stated Cobe France. "I love that Tige has an eye for the future and I'm excited to grow my career with them!"
Cobe is also sponsored by ProWake, O'Brien Wakeboards Australia, Nautilus Marine Insurance, Grundfos Pumps, Rubber Jungle Wetsuits, and O'neill.


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St. John's Karts & Kawasaki is a family owned business operating since 2000. We offer a wide variety of powersports products with top OEM's such as Kawasaki and Kymco. Also, we offer customized golf carts gas or electric from Club Car and EZGO. For the homeowner or commercial cutter, we offer lawn equipment from Cub Cadet and Toro. We are large enough to handle your needs, but small enough to know you by name.


In the last decade, over seven million CoolSculpting® treatments have been successful in helping bodies get rid of unwanted fat. This new, innovative procedure has become the number one slimming process for both men and women around the globe, and for good reason.
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The FDA has cleared CoolSculpting® as a safe medical procedure, so you can have peace of mind while undergoing this treatment. Another benefit is that the patient can get multiple areas treated. The treatment can be used on the abdomen, flanks, arms, back, and other areas.
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Trey @ The Palace 2/19/11 Download Available!
LivePhish.com has just made the 2/19/11 TAB show in Albany, NY show at The Palace Theater available on their site. Check it out; sadly it would appear that the code on my ticket does not seem to be redeemable for a free download like much of what LivePhish offers for Phish concerts; perhaps this is either in the works or an oversight. If you know, please give drop us an email if you have had any success.
Update: Per the folks at LivePhish.com there are NO free downloads of with this TAB tour. So, the code on your ticket stub means zilch!!! Such a bummer.
The show was simply incredible and if Trey is coming to your town AND you have tickets (cuz' there ain't no more left to git!) you will throughly enjoy yourself.
"I have a few friends here tonight," said Phish frontman Trey Anastasio at the Palace Theater in Albany last Saturday night. If by "few" he meant close to 3,000, he was right on. Smoke is still visible from the smoldering crater where the Palace once stood, thanks to Trey, along with his 7-piece band (collectively known as TAB, for the Trey Anastasio Band). They razed the venue to the ground on Saturday night, enthralling the sold-out crowd first with an acoustic set comprised of nearly all Phish songs, and then an electric set that was, well – electrifying.
Trey made a couple of references to being "home," (he did spend some time in Albany during his drug court appearances and community service tasks in 2008) and if home is where the heart is, it sure rang true on Saturday. Trey looked truly excited and grateful to be playing a relatively intimate show with his die-hard fans, pumping his fists and smiling ear to ear after every song.
The crowd sang along jubilantly during the first set, with the opener "Free" setting the tone, and groovy acoustic versions of Phish songs like "The Wedge," "Prince Caspian," and "Stealing Time from the Faulty Plan" followed. But the most poignant moment of the entire show, for me anyway, came during "Backwards Down the Number Line," which as a Phish song features prominent backing vocals. During Trey's acoustic version, which he introduced by saying he wrote it during his stay in Albany, the audience provided the backing vocals (with perfect timing, I might add). In essence, 3,000 crazed Phish-heads weren't just singing along with Trey – we were jamming with him. He sang his part, we sang the backing part. It created this amazing feeling of intimacy, of connection to the artist. And it continued with the next song "Limb By Limb," which featured a couple of back-and-forth vocal verses between Trey and the crowd; again, it was an incredible thing to be a part of. The most interesting reworking of all the Phish songs Trey performed that night was Guelah Papyrus, a weird little jazzy tune. Trey changed up the timing and structure of the song for his acoustic version; sometimes in the grand scheme of Phish, Trey's individual ability gets criticized because his songwriting now isn't anything like it was 20 years ago. But to rearrange an older song like Guelah into something fresh and interesting is a testament to how talented the man really is. The last four songs of the set saw other members of TAB filter on to the stage. Vocalists/horn players Natalie Cressman and Jennifer Hartswick joined Trey for the sappy but beautiful Wading in a Velvet Sea, which Trey dedicated to his longtime songwriting partner Tom Marshall, seated in the crowd; then keyboardist extraordinaire Ray Paczkowski joined the others for the older Trey solo song Black; and for the last two songs the rest of the band appeared – Tony Markellis on bass, Russ Lawton on drums and Russ Remington on sax and flute. They did a great version of the relatively new Valentine, and then closed the first set with an amazingly different version of The Devil Went Down to Georgia. Trey introduced the song as a "klezmer blues" song, referring to that fast-tempo music usually heard at Jewish celebrations. It was unclear what he meant until the song began – the fiddle part in the original song was covered by the horn section, and it truly did sound like klezmer music (see the video at the bottom). The crowd went crazy and we were all pumped for the electric set after the intermission.
And that set began with a bang – the grand horn-driven funk of Money, Love and Change whipped the crowd into a frenzy of dancing, as Trey and the band jammed it out for a good 10 minutes. After the straight-up blues of Done Did It, the band presented a rearrangement of the Phish tune Ocelot; it was an interesting version with the added horns, but overall it didn't add much to the original version. Then TAB pulled a crazy cover out of their bag of tricks, taking on the Gorillaz' Clint Eastwood. The band played it perfectly, with Hartswick easily handling the rap portions – the crowd went bananas. A scorching Night Speaks to a Woman followed that, with another extended funk-rock jam that pushed the energy level to the limit. The Toots and the Maytals song Sweet and Dandy came next, a cool reggae tune that was fun to hear, followed by the Five Stairsteps' Ooh Child, a somewhat boring version of a somewhat boring song. Going back to the reggae sound, TAB played the very rare Trey/Phish song Windora Bug, a quirky treat to hear. The other two highlights of the set were Sand and Push On Til the Day; TAB laid down a great groove for Sand and jammed it out extensively, while Push On brought the energy level to a new high, reaching a huge climax at the end of the long jam segment and sending the crowd into apoplexy.
The encore was Cayman Review, a solid funky tune that ended the show with the same enthusiasm as it began. All in all it was a fantastic show, and TAB seemed to be having a ton of fun, reflected by the singing and dancing of the audience. It's the vibe of a Phish show in a much smaller setting, creating a whole new experience.
This show gets 4.5 out of 5 stars!
At this time it can be officially said that Trey Anastasio and Classic Tab's show at The Palace is SOLD OUT! Sweet for us ticket holders, sucky for you lame-o's who waited until the last minute. Luckily, I'm sure you can scalp a ticket for around $120 the night of the show, ouch!
Last I checked there were only two shows (oddly both in Pennsylvania) that were still available for tickets, but all others are sold out as well. I'm very excited for this Saturday's show, I'm sure it will be well worth the wait.
Check back on monday for a full review of the show.
Hockey Night DJ at HiFi?
Personally there is nothing more satisfying than going to a hockey game, eating a few hotdogs, downing a few cold beers and of course the entertaining score that plays during intermission. Recently I was approached by one of the varsity hockey players at the prep school that I work at and was asked if I would DJ for their next rivalry.
I thought about it for about 2 seconds and said that I would love to, but there was one problem; I don't know if I had anything in my collection of music that would be geared towards hockey intermissions, warm up, penalities, etc. Of course songs that came to mind initially were Van Halens "Hot For Teacher", Rush's "Freewill" and "Tom Sawyer", and perhaps some Lamb of God, but I'm not sure I'm "with it" as the saying goes with the younger teenage hockey fan; actually I know that I'm not.
Well, after a few beers and some surfing on the web for hockey arena music I stumbled once again on a website that is the hockey DJ's dream of downloadable Mp3 files that fit just about any genre of hockey game, whether old timers like myself or wee little Mites and Squirts hitting the ice for the first time. The website is 2khockey.net and it has a well organized collection of both snippets for goals and brief time outs and also full length songs for quality filler.
Everything is free and you can preview the music before you download it; a good thing too since some of the songs do contain profanity and although you may not know it at the time, you certainly will get an ear full from the parent that will complain to who ever is above you, so be careful. I'm excited to DJ at the next hockey game and see if I can make these kids feel as if they are playing in the NHL; and perhaps gain a bit of "street cred" for my new found coolness factor.
Check it out and have fun by clicking here.
Ok, ok, so I couldn't resist with the passing of Gary Moore and my blurb about his playing with Cream alums Ginger Baker and Jack Bruce, that I had to post a very cool version of Politician they played in Germany on tour, check it out. Gary Moore was simply a madman jamming with these two geezers. I love the Ginger Baker but man does he look like the living dead all gaunt and missing teeth hitting the skins! I don't know who the dude is with the righteous flaming shirt that cameos a brief vocal part, do you?


Many states are in the process of developing plans for implementing a Comprehensive Child Welfare Information System (CCWIS). These next-generation systems offer improved integration, connectivity, and reporting capabilities. However, too many of the plans for implementation of these systems fail to put emphasis on the improvements in process and management systems that can dramatically increase capacity to serve. The requirements are instead focused on automating what is; providing expanded access to the same process, the same structures, and the same reports. You know the story. We put technology before workflow redesign, and we get a sophisticated system that tells us, in a better way, what we already know: We have massive caseloads and our clients are stuck in piles on caseworker's desks. When we get the process right, we have seen improvements such as 40 percent more clients served and 70 percent efficiency improvements for specific processes, and we know the same opportunities exist for states considering CCWIS.
1. Focus on process design first. CCWIS programs risk being technology-first efforts. At the outset, it is essential to take the time to reconsider how the work gets done, who completes it, how long it takes, the outcome, and, most important, how it is tracked. Too often there is a rush to move into screen configuration and design. But to be effective, two things should come first: human-centered process design and an effort to streamline processes. The use of human-centered design techniques, led by staff who understand the practice, is critical to ensure that capacity-driven innovation takes place. This approach challenges the casework process and identifies new ways to manage outcomes efficiently by considering all participants in the experience. Process streamlining identifies capacity opportunities focused on reducing the effort to produce quality work. If your project starts with system design, the opportunity for significant improvement has been missed.
2. Manage case flow over caseloads. Effective management of child welfare processes is often lacking in CCWIS project planning. Dashboards of caseloads, activities, and trends are all discussed and included in the procurement requirements, but the status of the work, what hinders progress, and who is needed to close out a task are rarely considered. Managing case fl ow across an agency requires careful assessment and planning of the supporting processes. With the right design you can track where the work is, identify bottlenecks, shift staff to where it will be needed, and make better hiring decisions. CCWIS can then provide the agency with the opportunity to control the case flow, rather than merely track the work.
The discussions in the market regarding modularity and agile development approaches have drowned out the critical focus on dramatically improving process outcomes.
3. Innovate data insights. There is considerable discussion regarding data analytics for child welfare, and predictive models remain controversial. But there are tremendous opportunities to leverage data to drive outcomes. This requires stepping back and evaluating how data are used as well as the impact and importance of that data in decision-making processes. When new data are identified, how is that data acted upon and by whom? What type of organizational structure would be best suited to analyzing and acting on the data? What new or additional data would help the agency better protect kids? Answering these key questions will enable the agency to determine whether and when caseworkers and supervisors would benefit from additional data support, as well as evaluate potential organizational changes that could facilitate more effective monitoring and analysis. For example, when educational outcomes change, or law enforcement actions occur in families, these data could alert a team to consider reassessment or inform the next review rather than solely rely on workers to notice the change in circumstance themselves.
By developing a plan that incorporates these suggestions into your procurement strategy, you are poised to harness the full potential of CCWIS. Even if CCWIS projects are underway, it isn't too late to take advantage of the benefits of a focus on capacity. Your agency will better manage case flow and deliver improved outcomes. Remember: While CCWIS innovations hold significant promise, driving improved outcomes isn't about development techniques. It's about an enduring focus on increasing capacity to improve the lives of the clients you serve.


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Police have filed charges against ousted leader Aung San Suu Kyi for breaching import-export lawsImage: Thet Aung/AFP/Getty Images
PoliticsAsia
Myanmar: Charges filed against Aung San Suu Kyi
02/03/2021 February 3, 2021
The ousted leader and several allies were detained in a coup just two days ago. G7 nations say they are "deeply concerned" by the leader's detention.
https://p.dw.com/p/3ooSN
Myanmar's police filed charges against ousted and detained leader Aung San Suu Kyi on Wednesday for breaches of the country's import and export law, according to a police document.
Police said she would remain in custody until February 15.
Military officers who searched Suu Kyi's residence found 10 hand-held radios that were imported illegally and used without permission, the document from a police station in the capital Naypyitaw said.
A separate document showed police filed charges against ousted President Win Myint for offenses under the Disaster Management Law. Reports say he is alleged to have broken COVID-19 rules during a campaign rally.
The charges against both politicians carry a maximum sentence of three years.
UN denounces military coup
UN Secretary-General Antonio-Guterres tweeted, "the detention of political leaders in Myanmar is a serious blow to democratic reforms in the country."
The UN Security Council held an emergency meeting Tuesday, but could not agree on a statement to condemn the coup. It requires China's support in order to be adopted, and China is Myanmar's main supporter at the UN.
"China and Russia have asked for more time," a diplomat told AFP, requesting anonymity.
Both China and Russia have sided with Myanmar amid criticism of its brutal treatment of Rohingya Muslims.
Myanmar's military arrested Suu Kyi, President Win Myint and several allies in a coup on Monday.
The army declared a one-year state of emergency. It said authorities had failed to resolve allegations of fraud in November's election. Suu Kyi's National League for Democracy (NLD) party won the vote by a landslide.
Suu Kyi has not been seen since her arrest. NLD party spokesman Kyi Toe said she was in good health at a separate location and would stay there for the time being. His comments cannot be immediately be confirmed.
Latest developments in Myanmar:
The NLD on Wednesday said its offices in several regions of the country had been raided, and documents, computers and laptops seized.
The raids started on Tuesday, the party said in a statement on Facebook.
It urged authorities to stop what it said were unlawful acts.
Myanmar's newly declared leader, General Min Aung Hlaing, said the military government installed after Monday's coup plans to carry out an investigation into alleged fraud in last year's elections.
The military government will also prioritize the COVID-19 outbreak and the economy, state newspaper Global New Light of Myanmar reported on Wednesday.
General Min Aung Hlaing led the coup against Aung San Suu Kyi's partyImage: MRTV/Handout/REUTERS
G7 slams military coup
The G7 nations and the EU said they were "united in condemning the coup in Myanmar," in a statement on Wednesday.
"We are deeply concerned by the detention of political leaders and civil society activists, including State Counsellor Aung San Suu Kyi and President Win Myint, and targeting of the media," foreign ministers from Canada, France, Germany, Italy, Japan, the UK and the US, together with the EU High Representative said.
The foreign ministers called on the military "to immediately end the state of emergency, restore power to the democratically elected government ... and to respect human rights and the rule of law."
People who are "unjustly detained" should be released, the lawmakers added.
Several of the G7 nations, including Germany and the US had already spoken out independently against the military takeover, ahead of Wednesday's joint statement.
Sanctions on the cards?
French Foreign Minister Jean-Yves Le Drian said that "additional sanctions will have to be considered at a European level" if the situation continues, in comments to French broadcaster Europe1 on Wednesday.
In 2018, the EU imposed sanctions against generals in Myanmarover killings of Rohingya Muslims. The EU also has an arms embargo on the Southeast Asian country.
China's Foreign Ministry on Wednesday said "relevant theories" that it supported or gave tacit consent to the coup "are not true."
"As Myanmar's friendly neighboring country, we wish that all sides in Myanmar can appropriately resolve their differences, and uphold political and social stability," Foreign Ministry spokesman Wang Wenbin said at a daily briefing.
Dr. Avinash Paliwal at University of London's School of Oriental and African Studies (SOAS) told DW that: "Wider Western sanctions will mostly hurt the people of Myanmar. The military elite will continue to have access to international finance and capital via China. This happened earlier too — and shall happen again if the West imposes stringent sanctions."
kmm,kbd/nm (Reuters, dpa, AP, AFP)
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