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

\begin{figure*}[ht]
\includegraphics[scale=1.0]{hist_color_combined.pdf}
\caption{\emph{Left:} redshift distribution of the selected galaxies. The dark histogram represents all the foreground galaxies from the Main Galaxy Sample of SDSS DR7. The quiescent galaxies from PG10 are shown in gray. The lightest colored unfilled histogram shows a distribution of the foreground galaxies that have at least one background galaxy within 150 kpc impact parameter. \emph{Right:} the color distributions of PG10 galaxies. Histograms of original PG10 colors (black), and $C_{\rm corr}$, (Equation \ref{cprimeab}; gray, filled), are shown for $u-g$ (top) and $g-r$ (bottom) colors. The expected reddening for Milky Way dust with an $A_v$ of 1, $R_v$ = 3.1 is shown by the black bar. The truncation used to excise extreme outliers is shown in vertical dashed lines.}
\label{galz_cdisp}
\end{figure*}

Galaxies process and return a significant fraction of their accreted gas to their surroundings, the circumgalactic medium (CGM) but the physical mechanisms involved as well as the matter distribution in this environment are still poorly constrained. Much of our knowledge of the distribution of baryons in

the CGM comes from absorption line studies which probe the gas phase. The interpretation of such measurements is often limited by our lack of knowledge of the ionization state of the gas. In this work we explore the distribution of dust around galaxies and use it as an alternative tracer of metals in this environment, independent of ionization corrections. It is important to realize that a substantial fraction of CGM metals might be in the solid phase. In the ISM, about 30\% of the metals are found in dust \citep{2001ApJ...548..296W}. Measuring dust reddening effectsfrom the CGM may also allow us to put constraints on the grain size distribution and potentially the mechanisms responsible for their ejection from galactic disks to halos, for example supernova explosions \citep{Silk1997,Efs2000} or radiation pressure \citep[e.g.][]{MQT2005,Salem2013}.

A number of authors have reported the presence of dust well beyond galaxy disks. Using superpositions of foreground/background galaxies, \cite{2009AJ....137.3000H} detected dust extinction up to about five times the optical extent of spiral galaxies. Using deep \emph{Herschel} observations, \cite{Roussel:2010dv} showed that emission from cold dust is seen up to 20 kpc from the center of M82. Using UV light scattered by dust grains, \cite{HodgesKluck:2014vn} reported the detection of dust up to about 20 kpc perpendicular to the disk of edge-on galaxies. With a statistical approach, \citet[][MSFR]{menard10} measured the cross-correlation between the colors of distant quasars and foreground galaxies as a function of the impact parameter to galaxies. They found an excess reddening signal on scales ranging from 20 kpc to a few Mpc, implying that the distribution of dust extends all the way to the intergalactic medium. \citet{2012ApJ...754..116M} showed that a similar amount of dust can been seen associated with strong Mg II absorbers at $0.5 < z < 2.0$, providing another line of evidence of the presence of dust on large scales around galaxies. \citet{Fukugita2011} showed that the summed contributions of dust in and outside galaxies appears to be in agreement with the total amount of dust that ought to be produced in the Universe. This implies that dust destruction does not play a major role in the global dust distribution and that most of the intergalactic dust survives over cosmic time.

In this work we focus on the low-redshift Universe and constrain both the amount of dust surrounding nearby ($z \sim 0.05$) galaxies and its dependence on galaxy properties. We do so by using a set of standard crayons, following the work of \citet{2010ApJ...719..415P}, i.e. galaxies for which the colors can be standardized. The outline of the paper is as follows: in \S \ref{obs} we describe the datasets how we estimate the color of a standard crayon galaxy. In \S \ref{methods} we introduce our estimator for reddening measurement, in \S \ref{aar} we present our analysis and results showing both detections of reddening and the variation of this reddening as a function of foreground galaxy parameters. We discuss these results in the context of galaxy formation and metal budgets in \S \ref{discussion}, and conclude in \S \ref{conclusion}.

\section{Data}\label{obs}

Our goal is to measure the mean color change of distant sources induced by the presence of foreground galaxies, as a function of impact parameter, $R$. Optimizing such a measurement requires both maximizing the number of foreground-background pairs and minimizing the possible scatter in the color distribution of the background objects. To do so we work with data drawn from the Sloan Digital Sky Survey \citep[SDSS;][]{york00}.

For our foreground population we select galaxies from the Main Galaxy Sample from the data release 7 \citep{strauss02} and use the magnitude limited selection $r < 17.77$. This produces a sample of 695,652 foreground galaxies for which two intrinsic properties are extracted from the MPA-JHU value-added catalog \citep{Kauffmann:2003iz, Brinchmann:2004hy}: specific star-formation rate (sSFR) and stellar mass ($M_\star$). The distribution of galaxies as a function of redshift is shown in the left panel of Figure \ref{galz_cdisp} with the black histogram.

For our background sample we make use of standard crayons, as introduced by \cite{2010ApJ...719..415P}: objects whose colors have a very narrow distribution. We select passively evolving galaxies from the Main Galaxy Sample (again, $r < 17.77$) using the criterion that they have neither detectable O{\sc ii} nor H$\alpha$ emission, significantly limiting their number. The details of that selection procedure are discussed in PG10. This provides us with a sample of 151,637 galaxies. We note that we do not exclude these galaxies from our foreground sample described above. The redshift distribution of the background galaxies is shown in the left panel of Figure \ref{galz_cdisp} in gray.

To estimate color changes we use the apparent model magnitudes of the galaxies and apply two corrections to them. First, we correct for the effects of Galactic dust reddening. To estimate them we avoid using the standard dust map from \cite{SFD98} which relies on FIR emission which is known to originate not only from the Milky Way but also from low redshift galaxies (see \citei{Yahata07}, \citei{Kashiwagi:2012we}, \citei{Peek:2013eh}, for a discussion of the effect). Instead, we emulate the work of \citet{Burstein:1982dz} and use a Galactic dust map based on the distribution of HI, as probed by the the Leiden-Argentina-Bonn radio survey \citep{Kalberla05}. We define the Galactic dust reddening $\Delta_{\rm MW}$, measured in the bands $a$ and $b$, in a given direction in the sky by
\begin{equation}\label{HIdust}
\Delta {\rm C_{\rm MW}} = \left(R_a-R_b\right) \frac{N_{\rm HI}}{7 \times 10^{21} \rm cm^{-2}},
\end{equation}
where $R_a$ and $R_b$ are the Galactic extinction coefficients for the SDSS bandpass filters \citep{Stoughton:2002dg}, and the ratio of reddening to H{\sc i}~ for this region is derived from \cite{2013ApJ...766L...6P}. We exclude galaxies with a measured $E\left(B-V\right) > 0.1$, where H{\sc i}~ column is known to be a poor reddening estimate, removing 1891 galaxies from our background sample. We note that using the \cite{SFD98} extinction rather than the method described above does not qualitatively modify our conclusions. Second, we need to remove possible trends between background galaxy colors and redshifts, which stem both from galaxy evolution and ``K-correction''. To do so we measure the median color-redshift relation for each of the 10 SDSS optical colors and characterize it using a fourth-order polynomial fit, refered to as $\Delta {\rm C_{\rm redshift}}$.

With these two correction terms in hand we finally define the corrected color of a galaxy by
\begin{equation}\label{cprimeab}
{\rm C_{\rm corr} = C_{obs} - \Delta C_{\rm MW} - \Delta C_{\rm redshift}}\;.
\end{equation}
This provides us with a distribution of corrected colors ${\rm C_{\rm corr}}$ for which the dispersion ranges from 21 to 180 millimagnitudes depending on the chosen bands. The right panel of Figure \ref{galz_cdisp} shows examples of such distributions.

\begin{figure*}[!ht]
\includegraphics[scale=0.8]{histo_zbuf.pdf}
\caption{Distribution of redshift differences for the galaxy pairs selected within 30 arcminutes. The light gray region shows pairs used for the direct dust reddening measurements. The dark gray region shows pairs used for the ``reverse test" used to characterize the effects of photometric bias, where the "background" galaxy is \emph{in front of} the ``foreground'' galaxy. The lightest gray area at the center represents pairs that are likely to be related in physical space ($| z_{\rm background} - z_{\rm foreground}| < 0.015$) and are thus not used in either measurement.}
\label{hzb}
\end{figure*}

\subsection{Outlier Rejection}

To increase the robustness of our statistical analysis we first remove outliers in the color distribution of the background galaxies (PG10, figures 2 \& 3). To do so we use Chauvenet's criterion, rejecting outliers that have larger deviations in color than would be expected for any points, given the standard deviation of the sample and the number of galaxies in the sample, in our case 4.35$\sigma$.  We reject galaxies that fail to meet this criterion in any of the 10 colors, which removes 7,861 galaxies from the sample, i.e. about 5\% of the data. We note that arbitrarily moving the threshold such that we reject half or twice the number of galaxies, or simply clipping at 3 $\sigma$ does not qualitatively effect our results. We also test against a bootstrap analysis and do not detect differences in the measured errors. Our extreme outlier rejection criterion is indicated as vertical dashed lines in the right panel of Figure \ref{galz_cdisp}. The final sample contains 141,885 standard crayon galaxies.

\section{Methods}\label{methods}

Given that the expected level of CGM dust reddening is lower than the intrinsic width of the corrected color distribution, we constrain its amplitude by measuring the mean color excess induced by the presence of foreground galaxies in a range of impact parameters, $\langle {\rm C}(R_{min},R_{max})\rangle$, where $R_{min}$ and $R_{max}$ are the minimum and maximum impact parameter. In addition to reddening by dust, apparent color changes can stem from other effects and systematic errors: physical correlations between foreground and background objects (galaxy clustering), distortions in the photometry due to the presence of a nearby galaxy and wide-field photometric errors. Below we define an estimator which takes those effects into account.

One requirement we put on our estimator is that it should not lead to any reddening signal if we measure the color changes of \emph{foreground} galaxies as a function of angular separation from background galaxies. Any such change would indicate our estimator is sensitive to some non-physical effect, as light coming from a galaxy in front should not be modified physically by a galaxy behind. We refer to this measurement as the ``reverse test".

\subsection{Physical and lensing-induced correlations}

Galaxies are known to follow a color-density relation \citep[e.g.][]{Blanton:2005eb} leading to mean color change as a function angular separation. To avoid being contaminated by such an effect, we impose a minimum redshift difference between our background and foreground objects. In Figure \ref{hzb} we show the distribution of foreground-background pairs within 30 arcminutes as a function of $\delta z = z_{\rm background}-z_{\rm foreground}$ for both the direct reddening measurement (right) and the reverse test (left; see \S \ref{sspe}). There is a sharp increase in the number of pairs on small scales, due to the clustering of galaxies. To be conservative we ignore galaxy pairs with $|\delta z| < 0.015$. Changing this value by a factor of 2 does not qualitatively effect our results.

Gravitational lensing increases the brightness of background galaxies behind foreground galaxies. Because of this brightening, there will tend to be more background galaxies brighter than a given threshold in the vicinity of foreground galaxies \citep{Narayan:1989bb}. The strength of this effect depends on both the gravitational magnification of the foreground population and the shape of the brightness distribution of the background sources. While our results are insensitive to background galaxy brightness, the average color of a population of galaxies will slightly change if the limiting magnitude is effectively altered. This effect, similar to the population reddening effect discussed in \cite{Peek:2013eh}, is very small; for our sample less than 20 millimagnitudes of color change per magnitude of brightening for all the colors we investigate. On scales of 150 kpc (about three arc\-minutes at the redshifts of interest), typical changes in galaxy brightness are $\sim 3 \times 10^{-3}$ and drop with scale roughly as $R^{-1}$ (Scranton 2005, MSFR).  We therefore expect lensing-induced color changes to be $\sim 5 \times 10^{-5}$ mag at R $\sim$ 150 kpc. This term is insignificant and we neglect it in the following.

\subsection{Wide-field photometric errors}

We expect wide-field variations in the photometry and colors at some level, as the SDSS survey was conducted over varying conditions over many years. This can be induced by calibration offsets \citep{Padmanabhan:2008js} or biases in the dust map \citep[e.g.,][]{2013ApJ...766L...6P}. Such large-scale variations may bias the color change we wish to measure: large scale structure in our foreground galaxies may overlap with regions of photometric error, generating a bias beyond simple Poisson noise. In order to mitigate this effect, we only focus on the excess color change measured with respect to a large-scale averaged mean color:
\begin{eqnarray}
\Delta {\rm C}(R_{min}, R_{max}) &=&
\langle {\rm C_{\rm corr}}(R_{min}, R_{max}) \rangle \\
&& \,-\, \langle {\rm C_{\rm corr}}(1\,\rm Mpc,2\,\rm Mpc) \rangle \nonumber
\end{eqnarray}
We find this effect to be typically of order $ 2 \times 10^{-4}$ magnitudes, and always smaller than our error bars and signal. We note that this method restricts us to measuring dust with $R < 1 $ Mpc and represents an imperfect mitigation of this very small effect.

\subsection{Small-scale photometric biases}\label{sspe}

On small scales, photometric estimation can be affected by the presence of nearby extended sources, like bright galaxies \citep{Aihara:2011kj}. The foreground galaxy is not a point source, and thus may have a real extended light distribution, or scattered light. The fact that the background object is also a galaxy introduces additional opportunities for error. To consistently measure the apparent magnitude of a galaxy, one must fit a model to the galaxy profile, which requires a careful estimate the sky brightness nearby. Any other galaxies in the same region of sky can bias the sky brightness estimate.

Quantifying such effects as a function of galaxy proximity and brightness requires tests of the SDSS photometric pipeline (see \citei{Huff:2013bc} and future work discussed therein). Instead of attempting to predict the amplitude of these effects, we can directly estimate them using the reverse test introduced above, i.e. measuring the color changes of \emph{foreground} galaxies as a function of angular separation from \emph{background} galaxies. Such a correlation should not lead to any signal. Therefore any measured quantity is an estimate of the amplitude of photometric biases. We perform a photometrically matched measurement $\Delta C_{\rm reverse}$.
To do so we weight galaxy pairs in the reverse test such that their pair-wise angular distribution matches that of the forward measurement. Our final circumgalactic dust reddening estimator is thus
\begin{equation}
\label{debias}
{\rm \Delta C_{\rm dust} = \Delta C - \Delta C_{\rm reverse}}\;.
\end{equation}
This small-scale photometric bias is expected to depend on the brightness of the foreground galaxies. Since the reverse test will tend to have higher redshift ``foregrounds'' than the dust measurement, we need take this difference into account. We estimate $\Delta C_{\rm reverse}$ as a function of the magnitude of ``foreground'' galaxies by binning the sample by quartiles in $r$ band magnitude. We find that, in practice, the strength of this small scale photometric bias is insensitive to whether we bin by quartiles or in some other way, and whether we use $r$ or another filter. A comparison of $\rm \Delta C_{\rm dust}$ and $\rm \Delta C$ is shown in the following section.

\section{Results}\label{aar}

\subsection{Mean reddening signal}\label{mrs}

\begin{figure}[!t]
\begin{center}
\includegraphics[scale=1.1]{loglog_ug.pdf}
\caption{Mean $u-g$ reddening excess measured as a function of scale, indicating the presence of dust in the CGM and IGM. The red line shows the best fit power law obtained by MSFR who measured the reddening excess induced by $z = 0.3$ galaxies on background quasars. Our analysis indicates, for the $u-g$ color, a higher level of reddening within 150 kpc and a departure from a power law. As shown in Fig.~\ref{color30--150} this excess is not seen in the other bands.}
\label{radialtrends}
\end{center}
\end{figure}

Using the color excess estimator presented in Equation \ref{debias} we measure the mean reddening induced by foreground galaxies for as a function of impact parameter, from 30~kpc to 1~Mpc. In Figure \ref{radialtrends} we show the radial profile of the $u-g$ color excess for 7 radial bins. We detect a reddening signal of about 10 milli-magnitudes at $R_p < 150$~kpc, which drops to about 1 millimagnitude at a scale of 1 Mpc. We attribute this signal to the presence of dust in the CGM and IGM. For comparison we show as a red line the best fit power-law trend to the results obtained by MSFR using foreground galaxies at $z\sim0.3$ and background quasars to measure colors. Overall, our results show a similar effect. This illustrates the power of standard crayons to perform low-level reddening measurements by reducing the intrinsic scatter in colors rather than increasing the size of the background sample. Our measurement also shows some differences with respect to the MSFR best fit trend. We observe an enhanced signal on scales ranging from 30 to 150 kpc.

\begin{figure}[h]
\begin{center}
\includegraphics[scale=.9]{colors_corr_new.pdf}
\caption{The average reddening of background galaxies with impact parameters between 30 and 150 kpc of all spectroscopic foreground galaxies. Solid black circles represent our dust reddening estimator $\Delta C_{\rm dust}\left(30~ \rm kpc, 150~ \rm kpc\right)$. An excess reddening is detected in all color combinations. The red lines represent the results of MSFR, assuming SMC dust. For reference, the empty gray circles show the results without the reverse test debiasing, $\Delta C\left(30~ \rm kpc, 150~ \rm kpc\right)$.}
\label{color30--150}
\end{center}
\end{figure}

In the regime $30$ kpc $<R_p<150$ kpc, where the signal-to-noise ratio of our measurements is higher, we can investigate the wavelength dependence of the measured color change. This is shown in Figure \ref{color30--150}. Our measurements show that the wavelength dependence of the signal is generally consistent with that of an SMC bar exctinction curve \citep[red dashes,][]{2001ApJ...548..296W} except at the shortest wavelengths. The $u-g$ color shows a significant excess, inconsistent with the SMC bar reddening curve, with a reduced $\chi^2$ = 7.6. We note that our $u$-band extinction is not affected by the canonical 2175\AA (NUV) absorption ``bump'' at the redshift of our foreground galaxies, i.e. $0.03<z<0.1$.

In general, small dust grains contribute to a steeper slope on the blue end of an extinction curve, generating an increase in $u-g$ reddening. To test the hypothesis that the increase in $u-g$ color relative to SMC extinction (Figure~\ref{color30--150}) is driven by the dust grain size distribution, we examine the very simplified case in which the dust has a single grain size and material. We do not expect that CGM grains are truly uniform, but we use this toy model as a simple test appropriate for our broadband data.

We investigate two extremely simplified dust models: graphite only and silicate only, each with a single variable grain size $a$.
We use dielectric constants given by \cite{Draine2003b}, \cite{DL1984}, and \cite{LD1993} and compute Mie scattering and extinction cross-sections using the publicly available \texttt{bhmie} code \citep{BH1983}.

While both the graphite and the silicate models show a best fit for smaller grains, $a_g = 0.05~\mu{\rm m}, a_s = 0.06~\mu{\rm m}$, both fall short of the u-band extinction, with reduced $\chi^2$ of 6.5 and 5.5, respectively. Therefore, we cannot conclude that we have strong evidence for a small grain population in the CGM. More likely, there exists some weak, unmodeled systematic that is increasing our errors. We also fit the data with the SMC curve but excluding the $u$-band and we find a better fit with reduced $\chi^2$=2.3. For the remainder of this work we exclusively refer to the simpler SMC dust assumption.

We can derive an overall CGM dust mass using
\begin{equation}
\label{dust-mass}
M_{\rm dust} = \int_{30~ \rm kpc}^{150~ \rm kpc} \frac{1.086\ A}{\kappa} 2 \pi r dr
\end{equation}
where $A$ is the extinction expected given the measured SMC reddening and $\kappa$ the SMC dust opacity. The fit both using and excluding the $u$-band data show a dust mass of $6 \pm 2 \times 10^7 M_\odot$; the fit is largely insensitive to $u$ as the $u$-band errors are large. These results are consistent with the result of MSFR, who found a CGM SMC dust mass of $5\times 10^7 M_\odot$.

\subsection{Trends with galaxy properties}\label{galprop}

\begin{figure}[h]
\includegraphics[scale=0.9]{histofg.pdf}
\caption{The bivariate distribution of foreground galaxies in sSFR and $M_\star$. The univariate quartile values are shown with long gray tickmarks; the splits used in \S \ref{galprop} are shown in black.}
\label{histofg}
\end{figure}

\begin{figure}[h]
\includegraphics[scale=1.0]{mass_ssfr_values_mod.pdf}
\caption{Average reddening between 30 and 150 kpc impact parameter of foreground galaxies, $\Delta C_{\rm dust}\left(30~ \rm kpc, 150~ \rm kpc\right)$, split into sub-samples by stellar mass (top panel) and specifc star formation (bottom panel). In the top panel the blue half-circles and errors represent the measurement of a sub-sample with average stellar mass of L* (the L* sample), while the red half-circles and errors represent the sub-sample with average stellar mass of 0.1 L* (the 0.1 L* sample). In the bottom panel the blue half-circles represent the high specific star formation rate sub-sample, at an average of 2 $\times 10^{-10}$ yr$^{-1}$, while the red half-circles and errors represent the low specific star formation rate sub-sample, at an average of 8 $\times 10^{-12}$ yr$^{-1}$. It is visually evident that the higher mass galaxies produce more reddening, but not ten times as much, as would be expected if CGM dust mass scaled linearly with galaxy stellar mass. No reddening trend is detectable as a function of sSFR.}
\label{overallmass_ssfr}
\vspace{0.5cm}
\end{figure}

\begin{figure}[!t]
\includegraphics[scale=0.8]{mass_ssfr.pdf}
\caption{The dependence of circumgalactic reddening on galaxy properties. The left panel shows the exponent $\beta$ characterizing the dependence on stellar mass $M_{\rm dust} \propto {M_\star}^\beta$, as a function of scale. The right panel
shows the exponent $\gamma$ characterizing the dependence on specific star formation rate $M_{\rm dust} \propto {sSFR}^\gamma$.}
\label{mass}
\end{figure}

Having access to a number of physical parameters for the foreground galaxies we can investigate correlations between the amount of dust in the CGM and galaxy properties. To do so we split the foreground sample by mass at $M_\star = 3 \times 10^{10} M_\odot$ (about 1/2 L*; see Figure \ref{histofg}). The average stellar mass of the low-mass group is $6 \times 10^9 M_\odot \simeq 0.1 $L* while the average for the high-mass group is $6 \times 10^{10} M_\odot \simeq $L*. We call these groups the $0.1$L* and L* sub-samples, respectively.

We determine the CGM reddening for each subsample and their ratios, shown in Figures~\ref{overallmass_ssfr} and \ref{mass}, respectively. In determining the ratio we make the explicit assumption that ratio of reddening to dust column is not a function of physical parameter by which we split the sample. We detect more reddening around L* galaxies over our fiducial impact parameter range (30-150 kpc), but only by a factor of $1.7_{-0.5}^{+0.7}$. If we assume a power-law dependence of CGM dust mass on host stellar mass we find
\begin{align}
\label{beta}
    &M_{\rm dust} \propto {M_\star}^\beta
    \rm{~~with~~}\beta = 0.23_{-0.15}^{+0.15}.
\end{align}
The ratio does not change significantly when we increase the range of impact parameter to 300 kpc, indicating that a more extended dust distribution around L* galaxies does not explain this weak dependence of CGM reddening with galaxy mass.
We rule out a linear proportionality between $M_{\rm dust}$ and $M_\star$ at a level greater than 4$\sigma$.

We repeat the experiment, splitting the galaxy population by sSFR at 3 $\times 10^{-11}$ yr$^{-1}$ (Figure~\ref{histofg}). The low sSFR subpopulation has an average sSFR of 8 $\times 10^{-12}$ yr$^{-1}$ while the high sSFR subpopulation has an average sSFR of 2 $\times 10^{-10}$ yr$^{-1}$. The trend with sSFR is characterized by
\begin{align}
\label{gamma}
    &M_{\rm dust} \propto {\rm sSFR}^\gamma
    \rm{~~with~~}\gamma = 0.04_{-0.09}^{+0.10}\;.
\end{align}
This is also reported in Figure \ref{mass}. It indicates that star forming and passively evolving galaxies around surrounded by a similar distribution of dust in their halo.

\subsection{Trends with disk angle}

Finally, we explore the spatial distribution of CGM dust as a function of position angle with respect to the major axis of the galaxy. To measure this, we first find a subsample of the target galaxies where the orientation of the major axis (position angle) of the galaxy is well measured. The SDSS photometric pipeline measures three position angles: the $\phi_{exp}$ of the exponential fit, the $\phi_{deV}$ of the deVaucouleurs fit, and the $\phi_{iso}$ of the best-fit ellipse to the 25 magnitudes per square arcsecond isophote. In cases where the galaxy's major axis is difficult to discern, these three fits will report essentially arbitrary values for $\phi$. To eliminate such cases, we consider only galaxies that have $|\phi_{iso} - \phi_{exp}| < 15^\circ$, $|\phi_{iso} - \phi_{deV}| < 15^\circ$, and $|\phi_{deV} - \phi_{exp}| < 15^\circ$, which is about 68\% of the total sample. We then measure the position of each background galaxy with respect to the $\phi_{dev}$ of the foreground galaxies to determine an azimutal angle $\delta\phi$ for each pair. Finally we bin the pairs into two groups: background sources probing the major axis region of the foreground galaxies ($|\delta\phi| < 45^\circ$) and those probing the minor axis region ($|\delta\phi| > 45^\circ$). We measure the ratio of reddening along the minor axis ($|\delta\phi| < 45^\circ$) to reddening along the major axis ($|\delta\phi| > 45^\circ$), as a function of impact parameter. We find an indication of an excess of reddening signal along the minor axis, excluding the null with 91\% confidence, compared to the major axis, on scales ranging from 30 to 50~kpc, shown in Figure \ref{phirat}. No significant difference is seen on larger scales.

\begin{figure}[!t]
\includegraphics[scale=1.2]{phi_ratio_mod.pdf}
\caption{The dependence of circumgalactic reddening on position angle around the galaxy as a function of impact parameter. The x-axis shows five radial bins from the forground galaxy, the y-axis shows the ratio of reddening seen in galaxies with a background along the minor axis to the reddening seen in galaxies with a background along the major axis. We only a faint signal within 50 kpc, excluding the null at 91\% confidence.}
\label{phirat}
\vspace{0.5cm}
\end{figure}

\section{Discussion}\label{discussion}

Characterizing dust reddening effects at a level below one percent is challenging. A number of effects unrelated to dust can bias the measurements: physical clustering, large-scale photometric variations, offsets in the estimation of the sky background level near extended sources, gravitational lensing-induced color changes due to possible brightness-color trends. In this analysis we have accounted for these effects by using an estimator sensitive the excess reddening as a function of angular separation and only accounting for color changes affecting background sources. Our results provide a new line of evidence that a substantial amount of dust resides in galactic halos. As opposed to previous statistical studies using quasars as background sources \citep[e.g.][]{Chelouche:2007dy,menard10} we have shown that it is possible to use background galaxies, and in particular standard crayons \citep{2008ApJ...688..198B,2010ApJ...719..415P}.

\subsection{The Spatial Distribution of CGM dust}

The increased reddening detected within 150 kpc (Figure \ref{radialtrends}) appears at first to be inconsistent with the smooth power-law found by MSFR.  However, the MSFR result assumes that all of the foreground galaxies are at $z = 0.34$.  As the MSFR results are based on photometrically detected foreground galaxies over a wide range of redshifts, we expect that any radial CGM edge in physical space would be washed out by the uncertainty in redshift.

The increased detection within 150 kpc is qualitatively consistent with absorption lines of highly ionized metals \citep{2009ApJS..182..378W} and cooler metals in the CGM \citep{Bordoloi:2011iu}. We find further similarity with gas-phase metals in the position angle distribution. The hint of increased reddening along the minor axis at low impact parameters is also consistent with previous work constraining the distribution of MgII absorption around galaxies \citep{Bordoloi:2011iu,2014arXiv1404.5301L}. These measurements of dust spatial distribution present an interesting and coherent picture to test against galaxy formation scenarios.

\subsection{Trends with Galaxy Properties}

A new frontier reached in this analysis is the ability to probe the relation between the amount of CGM dust and galaxy properties. Our results indicate that $M_{\rm dust, CGM} \propto M_\star^{\beta}$ with $\beta\sim0.2$ (Equation \ref{beta}). This trend provides us with a new constraint for the modelling of galactic winds \citep{Zu:2010ch,Oppenheimer:2006eq,Murray:2004jt} and metal pollution on large scales. We note that recent studies of CGM metals through absorption lines analyses also point out to a weak dependence between with galactic stellar mass \citep{Werk:2013ir,Zhu:2013bs}.

We note that the relatively weak relationship
between the amount of CGM dust and galaxy stellar mass
found in Equation \ref{beta} cannot persist to lower mass dwarf galaxies.
\citep[][;P14]{Peeples:2014fe} includes an analysis of the total mass of metals produced by galaxies as a function of mass. Extrapolating their relation -- that galaxies produce $\sim5\%$ of their stellar mass in metals (figure 1) -- we find that our Equation~\ref{beta} predicts more mass in CGM dust than is produced by a galaxy of $M_\star \simeq 5 \times 10^8 M_\odot$. This is of course unphysical; there must be some steepening of this relationship toward lower mass.

Lastly, the lack of detectable relationship between sSFR and CGM dust content has implications for dust lifetime in the CGM and feedback mechanisms. Our blue sample has a sSFR 25 times higher than the red sample, and yet we see no effect on the reddening from CGM dust. If dust is primarily ejected from galaxies by processes that are connected to star formation, it must survive for gigayears in the CGM to be equally represented around starforming and passively evolving galaxies.

\subsection{The Metal Budget}

\begin{figure}[h]
\includegraphics[scale=1.0]{mollyplot.pdf}
\caption{An accounting of all available metals as a function of galaxy mass, from the analysis of P14. Below the black line are metals in stars and the gas-phase ISM (purple), and ISM dust (orange). Above the black line are CGM metals: low-ions and OVI-traced metals (green) and CGM dust from this work (yellow). The hashed area represents metals missing from galaxies themselves. There is a very clear difference in the fraction of metals accounted for in 0.1 L* galaxies versus L* galaxies. For a discussion of uncertainties on these values see P14.}
\label{molly}
\end{figure}

Determining the location and state of metals can help us understand how galaxies produce and expel material, and therefore how they evolve. While early work highlighted the location of metals at high redshift \citep[e.~g.~][]{2007MNRAS.378..525B}, recently a complete analysis has been done by P14. This work determined the total mass of metals formed by a galaxy by $z \sim 0$ as a function of $M_\star$ that were not immediately locked in stellar remnants \citep{Fukugita:2004bf}: the ``available metals'' and discussed whether how much were detected within galaxy disks or in the CGM.

To illustrate the significance of CGM dust to this budget, we show a new version of P14 figure 9 including our measurement of the very weak dependence of CGM dust mass on host galaxy stellar mass (Figure \ref{molly}), under the assumption from \cite{menard10} that a galaxy of stellar mass $10^{10.4} M_\odot$ has CGM dust mass of $5 \times 10^7 M_\odot$. A number of assumptions go into this Figure which are discussed at length in P14. Importantly, P14 assumes no dependence of CGM gas-phase metal mass on $M_\star$ ($\beta = 0$). However, observations of OVI and lower ions can only rule out a linear, or stronger, dependence on $M_\star$ (rule out $\beta \ge 1$). Part of this uncertainty stems from the relatively few low-mass galaxies observed in the COS-Halos data set: only four in the range $4 \times 10^{9} M_\odot \lesssim M_\star \lesssim 10^{10}  M_\odot$ \citep{Tumlinson:2013cl}. Our dust work presents a more precise measure of $\beta$ (Equation \ref{beta}), in part due to the much larger range of foreground galaxy masses probed.

While each of these $\beta$ measurements are subject to various independent uncertainties and biases, the fact that all three measurements (OVI ions, lower ions, and dust) show weak dependence on $M_\star$ in this mass range suggests it is worth examining the physical implications. With these fiducial assumptions, a large fraction of the metals produced by 0.1 L* galaxies reside in the CGM, weakening any ``missing metals'' problem at that mass. Indeed, a 0.1 L* galaxy contains approximately as much metal in CGM dust as in the entire galaxy itself. Conversely, very little of the available metals from L* galaxies are found in detected phases of the CGM, suggesting that the missing metals must be in some unprobed phase or outside the CGM. These results give a valuable perspective on galaxy formation models, especially in the context of galactic feedback.

\section{Conclusion}\label{conclusion}

We can draw several conclusions from this work.
\begin{itemize}
\item Using galaxies and in particular standard crayons as background sources we detect the excess reddening induced by the extended distribution of dust around galaxies.
\item{We confirm the existence of $\sim 5 \times 10^7 M_\odot$ of dust in the CGM of 0.1 L* -- L* galaxies, consistent with the results of MSFR based on reddening of background quasars.}
\item We find a weak dependence of CGM dust reddening on galaxy stellar mass
$M_{\rm dust} \propto {M_\star}^{0.2}$ (Equation \ref{beta}), and no detectable dependence on specific star formation rate.
\item Including constraints on the distribution of metals from absorption line studies, the dust contribution to the overall metal budget indicates that the missing metals problem at low redshift is more acute near L* galaxies than near 0.1 L* galaxies.
\end{itemize}
We have found in this work that the photometry of close pairs of galaxies is susceptible to significant systematic error, even in a survey with photometry tested as meticulously as the SDSS \citep{Padmanabhan:2008js}. To press forward with the measurement of extragalactic dust reddening, we must build photometric pipelines that are resistant to the kinds of biases discussed in this paper. Future ground-based surveys and space missions may sidestep some issues with more stable seeing, darker skies, and higher resolution.  However, without a clear specification to deliver photometry unbiased by close neighbors, we cannot assume that such surveys will be optimal. Better bias constraints on the photometry of close pairs are also very important for weak lensing magnification measurements \citep{Huff:2013bc}. An alternative is to use observations of color-standardized point sources (quasars) to study extragalactic reddening.

With these important caveats in mind, we look toward the future of measuring dust in the CGM of galaxies with spectroscopic galaxy data. Expanding the analysis to a broader range of wavelengths would help better constrain the dust extinction properties, perhaps including WISE \citep{2010AJ....140.1868W} and GALEX \citep{2005ApJ...619L...1M} data. A preliminary investigation has shown much stronger systematic biases in close galaxy pairs when comparing photometry across surveys. Data from the GAMA survey \citep{Driver:2011gp} may help us reach higher precision, especially because the multi-pass spectroscopic survey avoids fiber collision issues, and many more close pairs can be studied. BOSS \citep{Dawson:2012fj} has observed ten times more passively evolving galaxies than the original SDSS data, but its targets are selected with cuts in color space, which may contaminate the standard crayons. If this contamination can be well understood, BOSS may allow us to study CGM reddening at $z \sim 0.5$. Future surveys like the notional high latitude survey proposed for WFIRST \citep{2013arXiv1305.5425S} may allow similar measurements toward $z \sim 2$, at the height of galaxy formation in the history of the universe.\\

\acknowledgements

We thank Daniel Rabinowitz of the Columbia statistics department for sage wisdom and Eric Huff and Genevieve Graves for insight into issues in the SDSS photo pipeline. We thank Jessica Werk for insight into COS-Halos mass dependence and Molly Peeples for providing the data from \cite{Peeples:2014fe} for Figure \ref{molly}.

JEGP was supported by HST-HF-51295.01A, provided by NASA through a Hubble Fellowship grant from STScI, which is operated by AURA under NASA contract NAS5-26555. BM is supported by NSF Grant AST-1109665 and work by LRC was supported by NASA Headquarters under the NASA Earth and Space Science Fellowship Program, grant NNX11AO09H.

Funding for the Sloan Digital Sky Survey (SDSS) and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, and the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web site is http://www.sdss.org/.

The SDSS is managed by the Astrophysical Research Consortium (ARC) for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, The University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, The Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington.

\bibliographystyle{yahapj}

redpajama_set_name: RedPajamaArXiv


This New EA Forex Black Star Premium hybrid Expert Advisor is able to trade in fully automatic mode or manage orders opened by the user!
In the auto mode, the EA finds the price consolidation areas. A position is opened once the price leaves such an area. If the position fails to be closed by a take profit and there was a crossing of the consolidation zone from the opposite side, the EA will open a locking position with an increased volume.
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In the third grid mode, the user opens a position using the panel (pending orders can be opened as well), and the EA builds up a grid for exiting the position.


On Friday the 27th February I gave a few online presentations (conferences) for the MoLeNET programme.
One was on images and photography in relation to mobile learning.
Presentation on images, creating images, editing images and using images on mobile devices. The use of images for teaching and learning with an emphasis on cameraphones.
This entry was posted on Tuesday, March 3rd, 2009 at 10:22 am and is filed under camera, flickr, images, molenet, n95, nokia, photo, photography, presentation, shozu, slideshare.	You can follow any responses to this entry through the RSS 2.0 feed. You can leave a response, or trackback from your own site.


text:
била је политичка позиција слична премијеру у влади старог Јапана током Нара и Хејан периода.

О позицији
Прва у истори забележена особа која је носила титулу даиџо даиџина био је син цара Тенџија, принц Отомо (касније цар Кобун). Уз ову титулу долазила је и велика политичка моћ али након неког времена, услед јачања клана Фуџивара, већ од 10. века особе са овом титулом нису имали права да одлучују осим ако се то није слагало са одлукама Фуџиваре. Иако је позиција под тим именом постојала (са прекидом) све до 1885, од 12. века се сматрала безначајном за веће политичке одлуке.
Након Меиџи обнове ова титула се накратко вратила. Санџо Санетоми је именован 1871. за даиџо даиџина али је ова титула ипак потпуно укинута 1885. у корист садашње титуле премијера Јапана.

Референце

Политика Јапана
Историја Јапана

redpajama_set_name: RedPajamaWikipedia


Meetings are held at 9:30 am the second Thursday of each month from September through May located at the Windermere Town Hall, 520 Main Street, Windermere, Florida 34786. Refer to the Meeting and Events Agendas to the far right for dates and details of each month's meetings.
Members are chosen alphabetically to bring 3 small floral arrangements (flowering plants acceptable) to the meetings for delivery to area nursing homes to be distributed to patients for their enjoyment. These arrangements are brought to the regular garden club meetings during the year. Other delivery arrangements are made during the summer. Refer to the Meetings and Events Agenda to the far right for dates and members scheduled to provide flowers for each month.
An ongoing project for garden club members is providing flowers each week for display in the Windermere Library. Members may provide an arrangement, a dish garden, a plant, or cut flowers in a vase. Please include a small card identifying the plant or flowers.
The plant or flowers need to be in the library on Monday after 10 am and picked up on Saturday before 5 p.m. Note that drop off for federal holidays are the next day. If you choose to purchase a plant or arrangement, please remove prices and vendor names.
Please check your assignment below and mark the date on your calendar. If you have a conflict, please exchange with someone on the list and notify the chairman. The chairman will remind members in advance via email or phone. Refer to the Meetings and Events Agenda to the far right for dates and members scheduled to provide flowers for each month.


The FNaFLore.com Forums are now archived. For more information, please see this post.
This site is not affiliated with Scott Cawthon. It is a fan site, that is attempting to find out the lore.
We at FNaFLore.com hope you enjoy your experience on this site, as well as all of the resources we've compiled.
If you spot any issues with our timeline, please send us an email via our Corrections page! We want to make sure the story is completely nailed down, and appreciate every correction thrown our way!


text:
Renting could overtake homeownership claims Savills
The private rented sector could overtake homeownership as the UK's dominant form of housing in the future, new research from Savills has claimed.
A combination of cultural and economic factors will be behind the switch while Savills predicts the number of private rented households in England and Wales will grow by 1.2 million by 2019.
Such growth would see the number of rented homes top the six million mark – some 24 per cent of the national total.
Changing views
While the rented sector grows, the number of owner-occupied homes is expected to fall by 200,000 to 14.67 million – 59 per cent of all households. These figures suggest that homeownership will remain the leading part of the housing market for some time yet, but Savills revealed that views towards owning a home are changing.
The younger generation in particular prefers to rent, and as they get older it is likely to mean that homeownership is no longer viewed as the norm.
Two-thirds of all households where the primary resident is under 35 years of age will be rented by 2019, equating to around 2.8 million homes – half a million more than the current figure.
Savills also predicts strong growth in the 35 to 49-year-old age bracket, with rented property in this sector expected to increase by 30 per cent or more than two million properties.
The rise in renting is expected to be most pronounced in London as an extra 250,000 households is expected to be rented by 2019. Rented housing would therefore account for 36 per cent of housing in the capital while owner-occupied properties are forecast to fall by 100,000 to 1.46 million and representing 42 per cent of London's homes.
The cost of living also has a large influence on people's decisions to buy or rent, the report claims as the number of people who can afford to buy is shrinking rapidly. These findings agree with a study from Ocean Finance that revealed many Brits between the ages of 25 and 34 are increasingly pessimistic when it comes to home ownership.
Among the reasons for the increase in buy to let are population growth, rising property prices, low wages and recent changes to mortgage lending criteria. While homeownership will remain the dominant force for some years yet, market trends suggest that renting could eventually overtake it to become the frontrunner.
See more buy to let news where One in five UK properties is owned by landlords.

redpajama_set_name: RedPajamaCommonCrawl


Star Wars: The Force Unleashed III is the non released and last game in the series. Sam Witwer. Knights of the Old Republic ist ein Rollenspiel, das rund 4.000 Jahre vor den Filmen spielt. Es behandelt einen Krieg zwischen der Republik Star Wars Legends, formerly known as the Expanded Universe (abbreviated EU), encompasses every.
Star Wars: The Old Republic is a massively multiplayer online role-playing game (MMORPG) based in the Star Wars universe. Developed by BioWare Austin Own your copy of Star Wars: The Force Awakens! Now on Digital HD and Blu-ray� Star Wars: The Old Republic, commonly abbreviated as The Old Republic, SWTOR, or simply Star Wars: Episode VII - The Force Awakens 3D Blu-ray (Collector s Edition) (2015): Starring Harrison Ford, Mark Hamill and Carrie Fisher. After the Battle of Endor.
Star Wars: Episode IV - A New Hope (1977) Trivia on IMDb: Cameos, Mistakes, Spoilers The official site for Star Wars, featuring the latest on Star Wars: The Last Jedi, Rogue One: A Star Wars Story, and Star Wars Rebels. Star Wars: Episode VII - The Force Awakens 3D Blu-ray (Collector's Edition) (2015): Starring Harrison Ford, Mark Hamill and Carrie Fisher. After the Battle of Endor. News, reviews, previews, tips, and downloads for multiple platforms. As filming begins today on the sequel to Fantastic Beasts and Where to Find Them, Warner Bros. has released summary which doesn�t tell us too much we didn�t.
Kotaku PC games and (sometimes) MMA reporter person. Mindless vessel for a sentient Star Wars: The Old Republic is a massively multiplayer online role-playing game . with the soundtrack which came with the Collector's Edition Star Wars the Old Republic Collector's Edition CD Soundtrack OST. Sorry If you must own the physical copy do not, do not, forget to download the rest online. The Music of "Star Wars: The Old Republic" Community Content. Dec 1, 2011 . The Collector's Edition of Star Wars�: The Old Republic� includes . all of the released tracks will be available for download Jan 8, 2013 When an upcoming MMO announces its collector's edition, the very first Star Wars: The Old Republic's CE included the soundtrack. but only half of it. little downloading know-how, I was able to piece together the SWTOR. Star Wars: The Old Republic Collector's Edition Soundtrack. Catalog Number: N/ A. Released On: December 20, 2011. Composed By: Gordy Haab, Jesse Harlin Star Wars: The Old Republic by Mark Griskey - Original Soundtrack review at Tracksounds. was released with the Collector's Edition of STAR WARS: THE OLD REPUBLIC, and another 30 pieces were released online for free download. Dec 20, 2011 Find a Unknown Artist - Star Wars: The Old Republic Collector's Edition ( Soundtrack) first pressing or reissue. Complete your Unknown Artist. Star Wars THE OLD REPUBLIC Collectors Edition PC w/ Sealed DARTH music CD of the soundtrack, and a book entitled "The Journal of Master Gnost- Dural.
Star Wars: Episode I � The Phantom Menace is a 1999 American epic space opera film written and directed by George Lucas, produced by Lucasfilm and distributed. Yes. The genius illustrator Jen Lewis has taken the two pinnacles of dinosaur entertainment�Jurassic Park and that disturbing �90s sitcom about prehistoric. Over the years, many critics have compared the game�s story to Star Wars, which is fair, because the game�s story is basically Star Wars. You�ve got a central. Download the free trial version below to get started. Double-click the downloaded file to install the software.


text:
Nashville.gov » Metro Clerk » Legislative » Legislation Details
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Bill BL2018-1306
An ordinance to amend Title 17 of the Metropolitan Code of Laws, the Zoning Ordinance of The Metropolitan Government of Nashville and Davidson County, by changing from R8 to SP zoning on property located at 926 West Trinity Lane, approximately 440 feet east of the intersection of West Trinity Lane and Old Buena Vista Road/Youngs Lane (1.30 acres), to permit up to 16 multi-family residential dwelling units, all of which is described herein (Proposal No. 2018SP-016-001).
NOW, THEREFORE, BE IT ENACTED BY THE COUNCIL OF THE METROPOLITAN GOVERNMENT OF NASHVILLE AND DAVIDSON COUNTY:
Section 1. That Title 17 of the Code of Laws of The Metropolitan Government of Nashville and Davidson County, is hereby amended by changing the Official Zoning Map for Metropolitan Nashville and Davidson County, which is made a part of Title 17 by reference, as follows:
By changing from R8 to SP zoning on property located at 926 West Trinity Lane, approximately 440 feet east of the intersection of West Trinity Lane and Old Buena Vista Road/Youngs Lane (1.30 acres), to permit up to 16 multi-family residential dwelling units, being Property Parcel No. 118 as designated on Map 070-07 of the Official Property Identification Maps of The Metropolitan Government of Nashville and Davidson County, all of which is described by lines, words and figures on the plan that was duly considered by the Metropolitan Planning Commission, and which is on file with the Metropolitan Planning Department and Metropolitan Clerk's Department and made a part of this ordinance as though copied herein.
Section 2. Be it further enacted, that the Metropolitan Clerk is hereby authorized and directed, upon the enactment and approval of this ordinance, to cause the change to be made Map 070 of said Official Zoning Map for Metropolitan Nashville and Davidson County, as set out in Section 1 of this ordinance, and to make notation thereon of reference to the date of passage and approval of this amendatory ordinance.
Section 3. Be it further enacted, that the uses of this SP shall be limited to a maximum of 16 multi-family units.
Section 4. Be it further enacted, that the following conditions shall be completed, bonded or satisfied as specifically required:
1. The development shall provide adequate access that meets the requirements of the Fire Marshal's Office and Department of Public Works.
2. With the submittal of the final site plan, provide architectural elevations complying with all architectural standards outlined on the Preliminary SP for review and approval.
3. The maximum height shall not exceed 49 feet measured to the roofline.
4. A standard "B" buffer shall be installed along the western and southern property lines. A standard "A" buffer shall be installed along the eastern property line and shall include additional evergreen vegetation in any areas where the setback is less than 5 feet.
5. All perimeter wood fencing shall consist of treated wood only.
6. Sidewalks and planting strip shall be constructed on all new public streets consistent with the requirements of Public Works. Sidewalks and planting strip shall be constructed along W. Trinity Lane consistent with the Major and Collector Street Plan.
7. All new internal public streets shall extend to the property lines.
8. The final site plan shall depict the required public sidewalks, any required grass strip or frontage zone and the location of all existing and proposed vertical obstructions within the required sidewalk and grass strip or frontage zone. Prior to the issuance of use and occupancy permits, existing vertical obstructions shall be relocated outside of the required sidewalk. Vertical obstructions are only permitted within the required grass strip or frontage zone.
9. The Preliminary SP plan is the site plan and associated documents. If applicable, remove all notes and references that indicate that the site plan is illustrative, conceptual, etc.
10. The final site plan shall label all internal driveways as "Private Driveways". A note shall be added to the final site plan that the driveways shall be maintained by the Homeowner's Association.
11. Comply with all conditions of Stormwater, Water Services, and Public Works.
Section 5. Be it further enacted, a corrected copy of the preliminary SP plan incorporating the conditions of approval by Metro Council shall be provided to the Planning Department prior to or with final site plan application.
Section 6. Be it further enacted, minor modifications to the preliminary SP plan may be approved by the Planning Commission or its designee based upon final architectural, engineering or site design and actual site conditions. All modifications shall be consistent with the principles and further the objectives of the approved plan. Modifications shall not be permitted, except through an ordinance approved by Metro Council that increase the permitted density or floor area, add uses not otherwise permitted, eliminate specific conditions or requirements contained in the plan as adopted through this enacting ordinance, or add vehicular access points not currently present or approved.
Section 7. Be it further enacted, if a development standard, not including permitted uses, is absent from the SP plan and/or Council approval, the property shall be subject to the standards, regulations and requirements of the RM15-A zoning district as of the date of the applicable request or application. Uses are limited as described in the Council ordinance.
Section 8. Be it further enacted, that this ordinance take effect immediately after its passage and such change be published in a newspaper of general circulation, the welfare of The Metropolitan Government of Nashville and Davidson County requiring it.
DeCosta Hastings
Download Bill BL2018-1306
Download Sketch for BL2018-1306
Download Site Plan for BL2018-1306
IntroducedAugust 7, 2018
Passed First ReadingAugust 7, 2018
Referred toPlanning Commission - Approved with conditions, disapproved without all conditions (9-0) on 06/28/2018
Planning, Zoning, and Historical Committee
Public Hearing Scheduled forSeptember 4, 2018
Passed Second ReadingSeptember 4, 2018
Passed Third ReadingSeptember 18, 2018
ApprovedSeptember 19, 2018
EffectiveSeptember 21, 2018
Requests for ADA accommodation should be directed to the Metropolitan Clerk at 615-862-6770.
Last Modified: 01/11/2019 12:00 PM


text:
Inventive colour: The art of Grace Cossington Smith
Posted by QAGOMA ● 2 May 2017
Grace Cossington Smith (1892–1984) was one of the most inventive colour painters to emerge from Australia's first wave of modernism in the early decades of the twentieth century.
Unknown / Grace Cossington Smith, c.1930–40 / 8522207 / Collection: Australian War Memorial, Canberra
Grace Cossington Smith, Australia 1892-1984 / Interior in Florence 1949 / Oil on board / 35 x 25.2cm (sight) / Gift in memory of Richard Harnett Cambridge and Merle Cambridge through the Queensland Art Gallery Foundation 2010 / Collection: Queensland Art Gallery | Gallery of Modern Art / © Estate of Grace Cossington Smith
After growing up in Sydney's northern suburbs, in 1914 Cossington Smith moved with her family to the Turramurra residence that would become her lifelong home and the centre of her creative production. She had already begun studying with the painter Antonio Dattilo-Rubbo, whose central Sydney studio became the site of much artistic experimentation during the interwar period. Though she travelled in Europe from 1912 to 1914, Cossington Smith claimed to have learnt the methods of Van Gogh, Cézanne, Gauguin and Seurat under Dattilo-Rubbo rather than overseas.
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Grace Cossington Smith, Australia 1892-1984 / The bridge in building 1929 / Oil on pulpboard / Gift of Ellen Waugh 2005 / Collection: National Gallery of Australia / © Estate of Grace Cossington Smith
Cossington Smith left Dattilo-Rubbo's studio in 1926, after which Sydney's light-filled harbour and the leafy terrains around Turramurra formed the main subjects of her art. Around this time the book The New Science of Colour (1915) by the American writer Beatrice Irwin fuelled Cossington Smith's interest in colour as a force capable of invoking the energetic undercurrents of her subjects. This is exemplified by her paintings of the construction of Sydney Harbour Bridge in the late 1920s, which form some of the most compelling examples of early Australian modernism.
Grace Cossington Smith, Australia 1892-1984 / Foxgloves growing 1929 /Oil on pulpboard / Private Collection / © Estate of Grace Cossington Smith / Photo: AGNSW/Jenni Carter
Grace Cossington Smith, Australia 1892-1984 / The window 1956 / Oil on hardboard / Gift of Graham and Judy Martin 2014, assisted by the Australian Masterpiece Fund / Collection: Art Gallery of New South Wales / © Estate of Grace Cossington Smith / Photo: AGNSW/Christopher Snee
While Cossington Smith worked in relative seclusion from her upper–North Shore home during the following decades, she was a regular contributor to group and solo exhibitions in Sydney. In the 1940s her work shifted in palette and tone to reflect the sombre hues and loose forms of Australia's native bush. She embarked on her last series of paintings in the 1950s, based on the rooms and spaces around her home. These interiors typify her desire to express 'colour vibrant with light'.
As a result of her solitude and self-effacing manner, Cossington Smith's work was not widely known until late in her career. She died aged 92 in 1984.
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Feature image detail: Grace Cossington Smith The window 1956
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CategoriesCategories Australian Collection CollectionTagsTags Grace Cossington Smith Making Modernism
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Finding joy in small things
Posted by Samantha Littley ● 1 Jun 2020


If you require RV transport services, you can rely on Show Car Transport to get your recreation vehicle to any place you need it to be – safely and securely. We provide door-to-door service and are dedicated to delivering the highest quality of service possible. With over 10 years of RV car transport experience, we will handle your motor home with care and professionalism.
RV transport may be necessary if you are traveling to a far away distance and plan to return with more passengers. Perhaps you're going over to Europe to explore their countryside; Show Car Transport will make sure your RV reaches your destination, even on the other side of the world.
All doors including cabinet doors and windows should be taped or tied closed. Antennas, propane gas bottles, should be removed and placed away from the unit. Take down all pictures and mirrors hanging or other loose and breakable items. No hazardous materials may be left in your RV during carriers, including gas or oil tanks, ammunition of any kind, or any other materials, which may be considered hazardous. Please ask your Show Car Transport if you are unsure. If you are ready to go, please fill out our carriers quote form to receive a quote for your move.
What forms of payment methods does Show Car Transport accept?
Show Car Transport will accept cash, credit cards, or certified funds for the deposit. The remaining balance is usually accepted in the form of cash or certified funds, unless other arrangements have been made. Please check with Show Car Transport to be certain of their payment policies.
What form of payment does Show Car Transport accept?
Does Show Car Transport transport Class A and Class C motor homes?
Class A motorhomes require driveaway services, unlike car transport travel trailers, Class B and 5th wheel trailers. At this time we do not offer driveaway service, which is when they must be driven to their destinations.
We at Show Car Transport recommend that you schedule your move as soon as possible to ensure that your RV is moved within the time frame which best meets your schedule. Traditionally, we are able to have a truck assigned and on its way to pick-up your RV 1 to 7 days from the date the RV is first available for pick-up.
How much will it cost to car carriers my RV?
Our carriers Specialists at Show Car Transport are trained to ask the right questions which pertain to your move. They will review your quote request and will accurately price your carriers.
long does it take to carriers a RV?
On average, a delivery of up to 500 miles will take 1 to 3 days - 1,000 miles will take 2 to 5 days - 2,000 miles will take 4 to 8 days, and coast to coast will range from 7 to 14 days with 10 days being close to the average. Please remember these are just estimated times for delivery. Our Dispatch Department at Show Car Transport will try to provide an accurate estimate of delivery as the truck assignment is made.
Remove all antennas, propane accessories, hazardous substances, and sheds from the RV completely and place away from the unit. Take down any hanging items on the walls i.e.: mirrors, pictures, etc. Remove or secure place settings, utensils, etc. PROPERLY secure all windows and doors by taping them from the outside or tie them down please include kitchen cabinets, drawers, and bathroom doors. Check and top off all fluid levels including transmission fluid, coolants, oil, wiper fluid and check for any leaks, repair all leaks prior to car transport. The most important RV safety precaution is to check all the tires air pressure if air is low please inflate them to correct pressure before car transport. Check lights to make sure they are all working. Make sure hitches; tow bars and any cables are securely fastened. Test the break system including the emergency break and service any brakes prior to car transport. Weigh your RV to make sure that it is not overloaded if the RV is overloaded the carrier will ask you to remove items and or charge you a fee for any excess weight at the car carriers discretion (see personal belongings). If the RV will be transport in subfreezing temperatures, prepare it as you would for winter storage, with water drained from plumbing systems and antifreeze in place.
What steps are involved in carriers my RV?
We at Show Car Transport only need a deposit to start your car transport. For your convenience we accept all major credit cards. The balance should be paid to the driver as they make the delivery. The remaining balance must be paid via Cash, Certified Check or Money Order (No Credit Card, Personal or Business checks, or any other form of payment will be accepted upon delivery). You may make payment in full, with a credit card; at the time the order is placed if necessary.


How many words for the numbers 1-10 in these different European languages can you correspond?
Four in Italian is not spelled with a c. It's "quattro."
That's now a type-in - thanks!
100% with 55 seconds to go!!!! BTW I can speak all of those languages as well as English, Mandarin, Cantonese, Japanese and Korean!!!
I thought expert would be some of the MUCH more obscure European-only languages, like Estonian or Catalan or Czech, not the same really-dang-common languages widely spoken outside of Europe with one or two harder-to-find ones.


text:
Rudge bezeichnet
 einen englischen Fahrrad-, Motorrad- und Automobilhersteller, Rudge

Rudge ist der Familienname folgender Personen:
 Dale Rudge (* 1963), englischer Fußballspieler
 Daniel Rudge (1840–1880), englischer Fahrradpionier und Radrennfahrer
 Humphrey Rudge (* 1977), niederländischer Fußballspieler
 John Rudge (* 1944), englischer Fußballspieler und -trainer
 Mary Rudge (1842–1919), englische Schachspielerin
 Olga Rudge (1895–1996), US-amerikanische Violinistin


text:
package com.sojostudios.as3;

import java.util.HashMap;

public class TestMap extends HashMap<String, String>
{

}

redpajama_set_name: RedPajamaGithub


The Core facility is designed to image both living and fixed material.
Imaging living cells or tissues: Adherent cells or tissue fragments can be imaged by a variety of methods depending upon the question being asked. If drug delivery is required, a perfusion style chamber is used; if gas exchange for the growth media is needed, glass bottom Petri dishes can be used; if long term (> 3 days) sterility is needed, there are sealed Rose chambers for imaging. Regardless of the experimental design, the specimen can be maintained from RT to 50ºC. Non-destructive image modes, i.e. phase contrast, differential interference contrast or polarized light, coupled with shutter and filtered illumination, provide as close to homeostatic conditions as possible.
Fluorescence imaging: Multiple labeled biomolecules such as GFP or fluorophore can be imaged in four-dimensions. This can be done over time (5th dimension) for live specimens as well as statically for fixed specimens. Specimens can be as thin as a single cell or as thick as a whole organism (e.g. Drosphilia). Conventional two-dimensional imaging can be done at high sensitivity, i.e. low bleaching rates. Three-dimensional imaging can be done in wide-field for relatively thin specimens or by confocal microscopy for thick specimens.
Image analysis: Once the images are collected, there is an extensive array of image processing and analysis software available to assist in data analysis and interpretation. These "tools" range from simple contrast manipulation to complex tracing and counting algorithms. There are also different forms of deconvolution available for "removing" the blur from fluorescent specimens, or transmitted light images. If multiple molecules are labeled, co-localization can be determined for either a static image or an image sequence. There are both automatic and semi-automatic 2-D and 3-D tracking/montaging algorithms available.


You and your colleague aren't quite seeing eye-to-eye, and you're eager to convince him to come over to your way of thinking. You're not trying to be stubborn and obstinate—you just know that your method is best, and you're determined to make him realize it.
Unfortunately, changing someone's mind isn't always easy. In fact, it can prove to be pretty difficult—particularly when you both feel strongly about your own opinions.
But, don't throw up your hands just yet! There are a few key phrases you can implement when presenting your argument that are sure to help sway the other person to your point of view.
When attempting to change someone's mind, it's all too easy to obsess over yourself and your own way of thinking. After all, you're the one who's right, and the whole point of this discussion is to prove that your way is best.
However, this self-centered approach results in a lot of "I", "me", and "you" language creeping into your spiel—which isn't necessarily an effective persuasion technique.
Instead, you're much better off using more collaborative language. Using words like "we" instead of "I" or "you" is a subconscious reminder that you're both on the same team—you're really just trying to find the best solution to a shared problem. Even better? It sounds less accusatory and demanding, which is crucial if you're attempting to facilitate a productive discussion.
What's one of my biggest pet peeve about political commercials? Candidates spend their precious airtime telling you all of the things their opponents won't do—and they neglect to even briefly mention what their own plans are.
However, many of us have the tendency to fall into this same trap when we're presenting our own arguments. So, remember that it's important that you place the majority of your emphasis on why your plan will work—rather than using all of your words and energy to explain why the other person's won't.
I know—it's all too easy to think that poking holes in another person's ideas and pointing out all of those obvious faults would be a surefire way to bring him or her to the light. However, this will likely only result in tension, arguments, and hurt feelings.
To be persuasive, you need to avoid being so negative and instead channel your time into explaining the benefits of your own idea. If you can point out all of the positives, you'll have a much better chance of changing someone's mind—without any hard feelings to boot.
Most of us aren't easily convinced—we aren't typically willing to drop our convictions at the first sight of a differing opinion. So, that usually means we require some specific examples and supporting evidence in order to change our minds about something we feel strongly about.
In fact, science shows that arguments that make use of specific examples are much more persuasive than those that only use vague terms and general assumptions.
This means that you should plan to follow up your assertion with a solid instance of when your suggested idea played out well. Different opinions aside—it's difficult to argue with facts.
We all have those experiences when we need to try to coax someone into seeing our point of view. And, unfortunately, you can't just snap your fingers and instantly change that other person's mind.
Persuading someone to kick his or her own opinions to the curb in favor of jumping on your bandwagon can take a little bit of strategy and thought. So, make use of these three key phrases, and you're well on your way to bringing that person over to your way of thinking.
Photo of courtesy of Hero Images/Getty Images.


Our offices is open Monday through Friday from 8:00 a.m. until 4:50 p.m. excluding holidays. We take our last walk-in customer until 4:50 p.m. every day. Our till closes at 4:00 p.m. each day and we accept documents until 4:50 p.m. but they are recorded the next work day.
Please call the Abstractor for an appointment. The cost to see the Abstractor starts at $5.00 and is $60.00 per hour. Call 269-945-1289 for an appointment (this includes attorneys, title companies, and examiners).
The public can now purchase copies from their office or home. You can log into the Register of Deeds Index Search - become register user and have your own ID and password. You then can search, save documents to your cart, purchase your documents with a debit or credit card, and print from your home or office. The cost is $1.00 per page for documents, plus a small service fee paid to Credit Card Merchant Service. The fee starts at $2.50 per purchase.
The duties and responsibilities of the Register of Deeds are recording, maintenance, and security of all real estate records for Barry County. We also assist customers with retrieving and obtaining copies of real estate records.
Effective March 24, 2017: On the last day of EVERY month the Barry County Register of Deeds Office will close at 4:00 p.m. We will accept no recordings after 4:00 p.m. on that last day of every month.
We take the last walk-in customer in the office at 4:50 p.m.
Effective October 1, 2016 in the State of Michigan: Regardless of the number of pages, all documents will cost $30.00 to record. This cost is inclusive of Michigan Remonumentation and Registers of Deeds Automation Fee. For a document that assigns or discharges more then 1 instruments $3.00 for each instrument assigned or discharged (in addition to the $30.00 flat fee) To certify a recorded document $5.00; copies remain at $1.00 per page and search fees at .50 cents for each year searched with a minimum of $5.00 – excepting tract index searches, contact the Abstract Office for fees.
An $ 80.00 deposit is required on all orders for new 40 year abstracts.
For Abstracts over 40 years, a larger deposit will be required.
An abstract left for comparison is the same as a deposit and will not be returned until the order is paid in full.
No credit can be extended; we accept Credit Card, Debit Card, and escrow account. Abstracts and searches not picked up within 6 months will become property of the Register of Deeds Office.


A hot day, with lots of competitive fun. Well done to Blue Mazarines House, overall winners this year!
Year 6 had a wonderful week on School Journey, Their days were packed with activities which included fossil hunting, a visit to Carisbrooke Castle, boat trip around the Needles and glass-blowing at Alum Bay. They also had lots of fun just playing on the beach!
The children had a great time experimenting with experiments during Science Week!
Our special World Book Day this year is Shakespeare themed. The children and staff came to school in some truly wonderful costumes and enjoyed great day of activities!
In January 2018, to start off our Shakespeare Literacy Project, the children in Years 2 to 6 visited The Globe Theatre to discover what it would have been like to watch one of his plays in the original theatre over 400 years ago. They had a tour then took part in fun and structured workshops.
A few photo's of our younger pupils in their wonderful Infant Nativity 'Prickly Hay', which was enjoyed by all.


text:
Fiat Sedici — легковий автомобіль (SUV). Спільна розробка італійського автовиробника Fiat та японського Suzuki (має назву Suzuki SX4). Виготовляється з 2006 року з кузовом хетчбек. Окрім передньоприводної версії є також повноприводна. Назва автомобіля з італійської мови перекладається як «шістнадцять». Основними конкурентами автомобіля є: Nissan Qashqai, Suzuki SX4 Hatchback і Skoda Yeti.

Зовнішній вигляд автомобіля досить незвичайний, а все завдяки своєрідній «ікластій» решітці радіатора, що віддалено нагадує Fiat Croma і ламаним фарам «бумеранг». Екстер'єром Фіат Седічі займалося відоме ательє ItalDesign на чолі з Джорджетто Джуджаро. Кузов кросовера має клиноподібну форму з ламаною підвіконною лінією, м'язистими передніми крилами і чітко окресленими задніми стійками. Седічі прикрашається пластиковим обвісом по периметру кузова, що робить його більш привабливим. Автомобіль оснащується 16-дюймовими колесами. Габарити Sedici рівні: довжина - 4115 мм, ширина - 1755 мм, висота - 1621 мм, колісна база - 2499 мм.

Двигуни

*В дужках показано витрати для повноприводної модифікації.

Виробництво

Примітки

Автомобілі Fiat


text:
Schizoprymnus tsymbalorum är en stekelart som beskrevs av Sergey A. Belokobylskij 1994. Schizoprymnus tsymbalorum ingår i släktet Schizoprymnus och familjen bracksteklar. Inga underarter finns listade i Catalogue of Life.

Källor

Bracksteklar
tsymbalorum


text:
La ciudad de Graneros se encuentra localizada en el sudeste de la provincia de Tucumán, Argentina. Es también la cabecera del departamento Graneros.

Población
Cuenta con , lo que representa un incremento del 19% frente a los  del censo anterior.

Granerenses destacados

 Axel Leonel Cordoba

Fiestas populares
 Festival de Doma y Folckore.
 Festival de la cumbia, cuarteto y guaracha.
 Fiestas patronales de la Virgen el 8 de diciembre.
 Festividad de San Pantaleón.

Parroquias de la Iglesia católica en Graneros

Referencias

Enlaces externos
 Coord. geográficas e imágenes satelitales
 Sitio federal

Cabeceras de departamento de la provincia de Tucumán
Municipios de 3ª categoría de Tucumán
Departamento Graneros


text:
CREATING A BACKWARD WONDERLAND
The more they do, the worse it gets - May 6, Daniel Ruth column
The column is funny and dead on. Mr. Ruth has nailed it.
This venal Legislature and governor have done more damage to this state in a single session thanks to the misguided zealots who voted them into office in November than any hurricane has ever done.
They have turned the whole state into a giant sinkhole. Or perhaps it is a giant rabbit hole a la Alice in Wonderland where everything is upside down. So laying people off creates jobs; environmental deregulation preserves our state's natural beauty; underfunding education improves our children's educational opportunities; making it harder to vote is good for democracy; mutual payoffs between lobbyists and legislators improves the moral climate in the capital; government intrusion into women's health issues fosters smaller government.
Welcome to our brave new world.
Sign a petition for the right to recall.
Mary Stephens, Largo
Why is Geronimo bad now?
While reading about our "elimination" of Osama Bin Laden, I noted that our native Americans were complaining about the Navy SEALs using the word "Geronimo." Does my memory fail me, or do I remember all our paratroopers in World War II calling out "Geronimo" when the bailed out of planes? It was okay for our military to use it then? But not now?
James Bardsley, Madeira Beach
Abortion legislation
Good for mother, child
Many people who have medical procedures and tests need and want as much information as they can to make an informed decision about how to proceed. This legislation will help give women of varying ages and maturity opportunities to avoid making an uninformed decision. Government intervention was accepted when women were given the right to choose to end their pregnancy. Now it seems that same intervention is unwelcome when the tables are turned.
This is really an effort to preserve the dignity of both mother and child who by all standards are unique living human beings by allowing every opportunity by receive and disseminate all information in regards to this decision.
B.A. O'Neill, Pinellas Park
Thanks, from Illinois
The Chicago Tribune reported May 5 that more than $186 million in federal money that Florida's Gov. Rick Scott turned down for high-speed passenger rail has been awarded to Illinois for improvements on part of the 110-mph corridor between Chicago and St. Louis.
Illinois' U.S. Sens. Dick Durbin, a Democrat, and Mark Kirk, a Republican, said the funds would increase travel speeds and create thousands of jobs. Thank you, Gov. Scott.
The taxpayers of Illinois appreciate your gift.
Don Evans, Barrington, Ill.
Alliance prevents deaths
In honor of Mother's Day, let us remember the children around the world who are not as lucky as us to have a healthy and safe childhood.
Globally, millions of children do not have access to vaccinations, a necessity we take for granted as a part of our childhood.
The GAVI alliance is a global program whose goal is to get desperately needed vaccinations to children. They have already prevented an estimated 5 million deaths through giving vaccinations. Two of the major killers of children in developing countries are diseases for which we now have vaccinations: pneumococcal pneumonia and rotavirus.
The GAVI Alliance can help prevent deaths, and it is imperative that the president and Congress support and invest in the program. This is such an easy way to prevent deaths around the globe, and it isn't even expensive. There is no reason that children around the world should die from these preventable diseases.
Robyn Schickler, USF medical student, Tampa
Terrorist still has hold on us
Dead or alive, Osama has won for as long as I need to show my passport at the Canadian and Mexican borders, suffer the indignity of being half- clothed and shoeless and patted down to fly, or wait far away from the gate for an arriving relative.
He still wins each time we spend our treasure and our nation's youth in pointless and distant wars, while being unable to fix our own highways and bridges, or heal our sick poor.
He is dead. When do we get our freedom back?
Maynard J. Hirshon, St. Pete Beach
Reckless, radical, wrong - May 9
Voters have already spoken
The headline is most appropriate to describe the first 21/2years of the Obama administration. The voters elected the Legislature and there was no secret what they wanted this election -nationally and statewise.
Richard W. Cope, Clearwater
More hurt for homeowners
The number of ways that the recently completed legislative session penalizes the average Floridian are to numerous to discuss in this forum.
However, as an economist, I feel compelled to point out the fallacy inherent in the passage of Senate Bill 1330.
This bill allows insurance companies to raise premiums, on a yearly basis, by up to 30 percent without government approval.
Republican lawmakers, bought and paid for the insurance industry, claim that by allowing premiums to rise, new companies will enter the market, which will eventually cause premiums to fall.
There are two problems with this theory.
One, insurance companies are not stupid. Even though collusion is illegal under antitrust laws, companies still collude, keeping prices artificially high and ensuring they continue to make healthy profits.
Two, this assumption of competition works only if both sides of the market are free to exit and enter. Consumers (the demand side) are forced to buy homeowners insurance if they have a mortgage. If the price set by the insurance companies is too high, we can't decline to buy their product.
Anyone with an ounce of common sense can see that this law tilts the market even more in favor of the insurance companies and penalizes Florida's homeowners.
Too bad our Legislature, and those who voter for them, don't have that ounce.
Joel Melvin, Clearwater
Vindication of the U.S. war on terror - May 8
A narrow escape in 1998
"Bin Laden declared war on us in 1998," according to columnist Charles Krauthammer. "But it was not until 9/11 that we took him seriously."
Krauthammer apparently doesn't believe that President Bill Clinton was serious when he ordered the Tomahawk cruise missile attacks that narrowly missed killing bin Laden on Aug. 8, 1998.
James Nelson, Largo
Up next:OSCEOLA'S DEMAREST OFF TO SOUTHEASTERN


Happy Birthday kurtie :D !!!
Or just a typing mistake ._.
How's life guys ??? xD I miss y'all !!!!!
Hey kurtieeeeeee!!! Nothing new... your still a nub and in still a noob.
It could be better than it is.
:< all I could was check the activity wall from time to time, I miss CC LIFE !!!!
I know your here kurtie.
O nu kurti I'll miss you but I'll be here for you when you come back.
Good job on winning the pink Easter umbrella kurti!! Very proud of you!!
Lucky. Atleast you have something to do rather than play.
"No one deserves to be alone"
Introducing the "Not Lonely Anymore Branch"
Thankkk chuu soo much guys ! >.
When you're good at drawing Anime and you see someone good at drawing realistic.
drawing is layf !!! I wish Im always like this, everyday >.
so close xD It's Kurt Mendes !
Ed are you dirty minded?


Switzerland has radioactive waste. Two-thirds of this waste originates from nuclear power plants, while medicine, industry and research account for one-third of the total. The waste is broken down into three categories: high-level radioactive waste (HLW), long-lived intermediate-level radioactive waste (LL-ILW) and short-lived low- and intermediate-level radioactive waste (L/ILW).
HLW consists of spent fuel assemblies from nuclear power plants and vitrified (glassy) residues from the reprocessing of the fuel assemblies. This waste produces a large amount of heat due to radioactive decay.
LL-ILW comprises waste from reprocessing (e.g. cladding tubes and endpieces of fuel assemblies) and intermediate-level operational radioactive waste from nuclear power plants and research facilities.
L/ILW consists mainly of operational waste from nuclear power plants and research institutions together with waste from medical and industrial applications. Additional L/ILW is also produced when nuclear power plants and research institutions are decommissioned.
Long periods of time will pass before the radioactivity of the waste has abated. As the beneficiary generation, we are already under an obligation to seek out and implement sustainable solutions for the management of this waste. The Swiss Nuclear Energy Act, NEA (Kernenergiegesetz, KEG) stipulates that all radioactive waste must be moved into deep geological repositories. According to the current time schedule, storage will not start before 2035. But even now, there is already a need for radioactive waste to be treated, placed in interim storage and transported.
According to the legislation, safe handling of the waste until the long-term management stage is the responsibility of the parties that produce the waste. As an independent supervisory authority, ENSI verifies whether the parties obliged to carry out waste management comply with the statutory regulations, and whether they take account of the latest international developments in science and technology. ENSI awards and coordinates research mandates in connection with regulatory safety research for the purpose of determining and expanding the current level of scientific and technical knowledge, so that this knowledge can be made available for supervisory tasks.
Two new members have joined the Expert Group on Deep Geological Repositories (EGT). With effect from 1 January 2018, the Swiss Federal Nuclear Safety Inspectorate, ENSI, is delighted to announce the appointment of Horst Geckeis and Neil Mancktelow as new members. Alan Geoffrey Milnes has stepped down from the EGT due to retirement.
ENSI, the Swiss Federal Nuclear Safety Inspectorate, has submitted the sixth Swiss national report to the Joint Convention on the Safety of Spent Fuel Management and on the Safety of Radioactive Waste Management (Joint Convention for short).
In the new position paper, 'Supervision of Deep Geological Repositories', the Board and Executive Board of the Swiss Federal Nuclear Safety Inspectorate (ENSI) express their opinions on, amongst other things, the division of roles between ENSI and those subject to the supervision.
During a joint project-workshop, members of the international BIOPROTA Forum and members of the IAEA MODARIA II Working Group 6 discussed methods for biosphere modelling within the context of deep geological repositories. The workshop took place from 10 – 12 May 2017 at the Swiss Federal Nuclear Safety Inspectorate (ENSI) in Brugg.
In future, the Swiss Federal Nuclear Safety Inspectorate, ENSI, will be able to calculate the amount of heat dissipated from transport and storage containers by means of a new independent calculation tool. This has emerged from ENSI's 2016 Research and Experience Report.
A lot of time elapses before the radioactivity of the waste wears off. As the generation benefiting from nuclear energy, we have an obligation to find and implement sustainable solutions for radioactive waste management.
This is the draft for the 2018 report to the Joint Convention on the Safety of Spent Fuel Management and on the Safety of Radioactive Waste Management.


text:
Audio Highlights Gallery
Press, Articles, and Interviews
Met Opera, Puccini: La Bohème
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Runs Oct 14, 2017 – Mar 10, 2018
The world's most popular opera returns in Franco Zeffirelli's classic production, with a series of exciting casts. Angel Blue, Anita Hartig, and Sonya Yoncheva (left) share the role of the fragile Mimì, with Dmytro Popov, Russell Thomas, and Michael Fabiano alternating as the poet Rodolfo. Alexander Soddy and Marco Armiliato share conducting duties.
Giacomo Puccini (1858–1924) was immensely popular in his own lifetime, and his mature works remain staples in the repertory of most of the world's opera companies. His librettists for La Bohème, Giuseppe Giacosa (1847–1906) and Luigi Illica (1857–1919), also collaborated with him on his next two operas, Tosca and Madama Butterfly. Giacosa, a dramatist, was responsible for the stories and Illica, a poet, worked primarily on the words themselves.
Production Franco Zeffirelli
Set Designer Franco Zeffirelli
Costume Designer Peter J. Hall
Lighting Designer Gil Wechsler
Revival Stage Director J. Knighten Smit
Latest Article:
Knowledge is Power…but a FRAMEWORK is Better
Jason Haaheim | March 31, 2019 April 6, 2019 | Art & Aesthetics, Composers, Deliberate Practice, Excerpts, Opera, Process of Auditions, Science & Music, Timpani
(The Attributes of Deliberate Practice: A Framework of Domain-Specific Knowledge) How many numbers in a row can you memorize? Maybe it's a weird question, but have you ever tried to memorize a really long string of digits? Try it. We'll start with something reasonably short. How about this? 3 1 4 1 5 9 2 6 5 3 5 8 9 7 9 Stare at that sequence of numbers for a moment, memorize them, then turn away from your screen and try to recall them in order…. (Go ahead. I'll wait.) […]…
Artful Timpani Auditioning
Tuesday 10:00AM
Wednesday 10:00AM
Thursday 10:00AM
National Youth Orchestra Coaching
© 2019 Jason Haaheim. All rights reserved.
Photos: Justin Haaheim | Powered by The Venture Platform.
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text:
The Godskins are one of the most terrifying creatures in Elden Ring. You can fight them and take their weapons and armor, but did you know that you can also get their prayerbook?
Getting the Godskin Prayerbook gives you the power to wield the black flame – a powerful spell meant to eliminate gods and demigods. If you want to strengthen your Faith build or become part of the Godskin, then you'll want to consider getting this book.
Prayerbooks are useful for sorcerers and players who enjoy using spells in their adventures. As of now, there are 101 incantations in Elden Ring. There is a plethora of ways to obtain spells in the game such as purchasing them from vendors or looting them in various areas of the map.
What is the Godskin Prayerbook In Elden Ring?
Godskin Prayerbook Location
How to Use Godskin Prayerbook In Elden Ring
Elden Ring Godskin Prayerbook Uses
1. Black Flame
2. Black Flame Blade
However, if you want to unlock the secret ones, you'll need a prayerbook. This guide tells you everything you need to know about the Godskin Prayerbook in Elden Ring, from its history, where you can get it, to what it does.
The Godskin Prayerbook is a special item that unlocks two dark incantations: Black Flame and Black Flame Blade. It belonged to the Godskins, who are humanoids that serve the Gloam-eyed Queen.
The Gloam-eyed Queen raised the Godskins to become god hunters, and she herself wielded the power of Destined Death. With the Black Flame, she could manipulate Destined Death and bring death to inhabitants of the Lands Between, gods, demigods, and even Tarnished.
However, it was locked away by Queen Marika. After her defeat, the power of the black flame was rendered useless against the demigods.
We never meet the Gloam-eyed Queen as her identity remains a mystery, but despite her absence, we know that she made a huge impact as the Godskin continue to roam the Lands Between.
If you want to get the Godskin Prayerbook, it can be found in Stormveil Castle. Specifically, an underground cellar near the Liftside Chamber site of grace. If you've defeated the boss Margit the Fell Omen, then you already have access to this castle.
Here is a step-by-step guide on how to get the Godskin Prayerbook:
Go to the Rampart Tower site of grace, a place surrounded by explosive barrels.
Exit through the door and head east, where you'll see a roof.
Jump onto the roof. This might take a few tries, just make sure to do a sprinting jump. If you fail, you can always try again using the site of grace.
Once you drop on the roof, look to your left and find a safe spot to jump mid-way before landing in the inner courtyard to avoid dying from the fall.
Right away, you will see a door that leads you to the underground cellar straight ahead. Go down the stairs and into the tunnel.
Be warned, there are lots of rats you'll have to fight here.
If you want to get past the fog wall, you'll need the Stonesword Key. This item can be purchased from various merchants and looted in multiple locations. You can also find it in multiple areas in Stormveil Castle. The nearest one can be looted from a corpse inside a building with a broken roof, which can be accessed from the tip of the Rampart Tower.
When you enter the fog wall, there's a chest on the right side of the room that has the Godskin Prayerbook inside. You can also snag the Godslayer's Seal in the second chest, which is also useful for Black Flame incantations.
Alternative: If you want to start from the Left side Chamber site of grace, you can run through the courtyard and hug the right wall until you find the set of stairs leading down.
However, this path is much more difficult as enemies will follow you into the cellar.
Now that you have the Godskin Prayerbook, you can go to Brother Corhyn or Miriel, Pastor of Vows to unlock the spells inside it. Pastor Miriel is the easiest to find, as he is an old turtle that stays in one place: the Church of Vows.
If you've killed him, then you'll have to go to Brother Corhyn. He can be found in these locations:
The main room of Roundtable Hold
Altus Highway Junction site of grace
Altus Plateau
On a cliff outside the Colosseum with Goldmask
On a bridge located southeast of the Stargazer's Ruins, in the Mountaintop of the Giants
Leyndell, Ashen Capital.
Giving the Godskin Prayerbook to a cleric unlocks two dark spells: Black Flame and Black Flame Blade.
The Black Flame is a spell that throws an explosive black fireball, dealing fire damage upon impact. Enemies that are attacked with it lose 2-5% of their HP. Purchasing it costs 7,500 Runes and it requires you to have 20 Faith to cast this spell. The Black Flame also costs 25 stamina and 18 FP.
The Black Flame is a spell that wraps your right-hand weapon in black flame, increasing the weapon's damage. Enemies that are attacked with it lose 2% of their HP. Purchasing it costs 6,000 Runes and it requires you to have 17 Faith to cast this spell. The Black Flame also costs 10 stamina and 15 FP.
That's all for our guide on the Godskin Prayerbook in Elden Ring! Prayerbooks are pretty tricky to find in the game, which is why we wrote this guide.
If you managed to find this prayerbook and unlocked the spells within it, congratulations! You can try out these spells in your next adventures and see if they were worth it. If you're not satisfied, there are a lot more prayerbooks and spells you can find scattered throughout the game.
For more guides on prayerbooks in Elden Ring, you can check out the rest of our articles here.
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