text:
\section{Introduction}

The isotopes of the elements located in Mendeleyev's periodic table beyond the iron group ($Z >$ 30, hereafter, heavy elements) are synthesized in neutron-capture nuclear reactions (Burbidge et al. 1957), which are subdivided into slow ($s$-) and rapid ($r$-) process of neutron-captures, depending on the neutron flux density. The
$s$-process is divided into two components, depending on its site and the production efficiency of isotopes of
various masses ($A$). The main component is associated with the thermally pulsing asymptotic giant branch (AGB) phase of intermediate mass stars and the production of isotopes with $A$ = 90-208. As confirmed by theoretical and observational studies (for a review, see Busso et al. 1999), stars with initial masses of
1-4 $M_\odot$ made the greatest contribution to the solar abundance of $s$-nuclei. The weak component runs
in massive stars ($> 10M_\odot$) at the core helium burning stage and produces the lightest isotopes of heavy elements, with $A \le$ 90 (see, e.g., K\"appeler et al. 1989).

The $r$-process overcomes the barrier near bismuth ($Z$ = 83, $A$ = 208) and can synthesize the heaviest nuclei. It is probably associated with more than one type of stars. The models of neutron star or black hole mergers, type II supernova explosions, accretion-driven gravitational collapse, etc. are proposed in the literature, and so far there is no general consensus (Nishimura et al. 2017). However, all agree that the $r$-process must occur in stars more massive than those in which nucleosynthesis proceeds in the main component of the $s$-process. The point is that different elements and different isotopes of the same element are synthesized with different efficiencies in the $s$- and $r$-processes. For example, in Solar system matter 80\,\%\ of the barium are the $s$-nuclei synthesized in AGB stars, while europium is a product of predominantly the $r$-process, by 94\,\%\ (Travaglio et al. 1999). Barium ($A$ = 134-138) and europium ($A$ = 151, 153) cannot be produced in the weak component of the $s$-process. Back in the late 1970s Galactic halo stars were shown to exhibit europium
overabundances relative to barium relative to the corresponding solar ratio, i.e., [Eu/Ba]\footnote{We use the standard notion for elemental ratios: [X/Y] = log$(N_X/N_Y)_{*}$  -- log$(N_X/N_Y)_{\odot}$.} $> 0$ (Spite
and Spite 1978). This is possible only if the $r$-process proceeds in stars with a shorter evolution time, i.e., more massive than AGB stars. Theoretical arguments for the dominance of the $r$-process over the $s$-process at the formation epoch of the halo stellar population were advanced by Truran (1981).

To solve the problem of the astrophysical site for the $r$-process and to refine the present views of the chemical evolution of the Galaxy, it is very important to reconstruct the history of enrichment of Galactic
matter with $s$- and $r$-nuclei. The [Eu/Ba] ratio is a good indicator of the ratio of the contributions
from the $r$- and $s$-processes ($r/s$) to the barium abundance at the epoch when the star was formed. If the $r$-process dominated, then the star has [Eu/Ba] = [Eu/Ba]$_r$, which in different works on calculating
the contribution from the main component of the $s$-process to the solar europium and barium abundances varies from 0.67 (Travaglio et al. 1999) to 0.80 (Bisterzo et al. 2014) and is 0.63 in the theoretical waiting-point (WP) approximation (Kratz et al. 2007). Mashonkina et al. (2003) showed than in thick-disk and halo stars [Eu/Ba] lies in the range from 0.35 to 0.67 and nucleosynthesis in AGB stars had already begun at the formation epoch of the thick disk. The contribution of the $s$-process to the barium abundance was estimated to be from 30 to 50\,\%, and the thick disk was shown to have been formed in the
interval between 1.1 and 1.6~Gyr from the onset of protogalactic collapse. Having analyzed the ratios
between Ba, La, Nd, Eu, and Dy, Burris et al. (2000) concluded that the contribution of AGB stars becomes
noticeable starting from [Fe/H] = $-2.3$. Simmerer et al. (2004) lowered this boundary to [Fe/H] = $-2.6$ by analyzing the La/Eu ratio, while Roederer et al. (2010), on the contrary, raised it to [Fe/H] = $-1.4$ based on Pb/Eu observations.

Another indicator of $r/s$ in the barium abundance is the fraction of isotopes with an odd mass number, $f_{\rm odd}$. In Solar system matter barium is represented mainly by five isotopes with the following fraction in
the total abundance: \iso{134} : \iso{135} : \iso{136} : \iso{137} : \iso{138} = 2.4 : 6.6 : 7.9 : 11.2 : 71.7 and $f_{\rm odd}$ = 0.18 (Lodders et al. 2009). A different mixture of isotopes is produced in the $r$-process; for example, Travaglio et al. (1999) predicted \iso{135} : \iso{137} : \iso{138} = 24 : 22 : 54 and $f_{\rm odd,r}$ = 0.46. A close value is obtained in the WP model: $f_{\rm odd,r}$ = 0.438 (Kratz et al. 2007). The
Ba~II 4554 and 4934\,\AA\ resonance lines are sensitive to a variation of the mixture of barium isotopes, and this makes it possible to determine $f_{\rm odd}$ and, hence, $r/s$ in stars.

Two methods of determining $f_{\rm odd}$ are used in the literature. Both are based on the fact that for the
isotopes \iso{135} and \iso{137} there is hyperfine splitting (HFS) of levels and each barium line consists of a set of components. The first method uses the fact that the width of the Ba~II 4554\,\AA\ resonance line increases with $f_{\rm odd}$. This method requires a very high spectral resolution ($R$) and a superhigh signal-to-noise ratio ($S/N$). For example, for the nearest ($d$ = 62 pc) halo star, HD~140283, Lambert and Allende Prieto (2002) took a spectrum with $R\simeq 200\,000$ and $S/N\simeq 550$, while Gallagher et al. (2010) took a spectrum with $S/N\simeq 1\,110$ (!). The complexity of the method is related to the necessity of separating the line broadening due to the hyperfine structure from the broadening by rotation, macroturbulent motions in the stellar atmosphere, and the instrumental broadening. In the classical approach (homogeneous and 1D model atmospheres) lines in adjacent spectral regions, as a rule, of iron-group elements are used for this purpose. The weakness of this approach is obvious. Whereas the instrumental and rotational broadenings produce
the same effect on lines with close wavelengths, the effect of macroturbulence can depend on the line
formation depth. It cannot be properly taken into account for the Ba~II resonance lines using the (predominantly subordinate) lines of other elements. That is why the results of different authors for the same star
differ so much. For example, for HD~140283 Lambert and Allende Prieto (2002) obtained $f_{\rm odd}$ = 0.3$\pm$0.21, which points to a significant contribution of the $r$-process to the barium abundance, while Gallagher
et al. (2010) gave $f_{\rm odd}$ = 0.02, which is lower than that in a pure $s$-process: $f_{\rm odd,s}$ = 0.11 (Arlandini et al. 1999). The results obtained by Gallagher et al. (2015) with the application of hydrodynamic
calculations in a 3D model atmosphere are encouraging: $f_{\rm odd}$ = 0.38 for the same star, which is consistent with the present views of the history of heavy-element production in the Galaxy. However, it is unlikely that the method will be widely used, because it is impossible to obtain the observed spectra of the required
quality for metal-poor stars, which are mostly at great distances.

The second method uses the fact that the HFS effect is different for the Ba~II resonance and subordinate
lines. First, the total barium abundance is determined from the subordinate lines and then $f_{\rm odd}$
is varied until the same abundance is deduced from the resonance lines. The idea was proposed by Magain
and Zhao (1993), but it was used very rarely. The method does not require a superhigh quality of
the observed spectrum, but it requires an accurate determination of the atmospheric parameters, especially
the microturbulence ($\xi_t$), and abandoning the LTE assumption in Ba~II line calculations, because
the non-LTE effects are different for the resonance and subordinate lines. Therefore, the method was
applied for a small number of stars and predominantly in our papers: Mashonkina and Zhao (2006, 25 stars), Mashonkina et al. (2008, 2 stars), and Jablonka et al. (2015, 2 stars).

The goal of this paper is to determine the relative contribution of the $r$- and $s$-processes to the barium
abundance in four halo giants by determining the fraction of odd barium isotopes from an analysis of
the Ba~II resonance and subordinate lines. Our study is motivated by two factors. First, the parallaxes
measured by the Gaia observatory were published in April 2018 (Gaia Collaboration 2018), which allow
accurate surface gravities (log~$g$) to be obtained for stars up to $\sim$2.5 kpc away. Second, quantum-mechanical calculations of Ba~II + H~I collisions were performed for the first time in 2018 (Belyaev and
Yakovleva 2018). Using these data in non-LTE calculations will allow the degree of confidence in the
results obtained to be increased.

\begin{table*}
\caption{Atmospheric parameters of the selected stars and characteristics of observed spectra. $\xi_t$ is in km\,s$^{-1}$.}
\label{tab:param}
\begin{center}
	\begin{tabular}{rcccclcl}
		\hline\hline
		\multicolumn{1}{l}{HD}  & $T_{\rm eff}$ & log\,$g$ & [Fe/H] & $\xi_t$ & \multicolumn{3}{c}{Spectra} \\
		\cline{6-8}
		  &  K    &      &        &    & Spectrograph & R & Ref. \\
		\hline
		  2796 & 4880 & 1.80$\pm$0.03 & $-2.19$ & 1.8 & VLT2/UVES & 70\,000 &  ID: 076.D-0546(A) \\
		108317 & 5270 & 2.81$\pm$0.02 & $-2.24$ & 1.4 & Magellan/MIKE & 60\,000 & Ezzeddine (2017) \\
		122563 & 4600 & 1.40$\pm$0.02 & $-2.57$ & 1.6 & VLT2/UVES & 80\,000 & Bagnulo et al. (2003) \\
		128279 & 5200 & 3.00$\pm$0.01 & $-2.19$ & 1.1 & VLT2/UVES & 45\,000 &  ID: 71.B-0529(A) \\
\noalign{\smallskip}\hline \noalign{\smallskip}
	\end{tabular}
\end{center}
\end{table*}

The sample of stars, observational data, and atmospheric parameters are presented in Section~1. The
non-LTE calculations for Ba~II are presented in Section~2. We determine the barium and europium abundances
in Section~3 and the fraction of odd barium isotopes in Section~4. Our conclusions are formulated
in Section~5.

\section{SAMPLE OF STARS, OBSERVATIONAL DATA, AND ATMOSPHERIC PARAMETERS}\label{Sect:stars}

The formulated problem requires a very high accuracy of determining the barium abundance from
individual lines. Therefore, we exclude the blended Ba~II 4934 and 6141\,\AA\ lines and use three lines:
one resonance, Ba~II 4554\,\AA, and two subordinate, Ba~II 5853 and 6497\,\AA, lines. To choose the stars,
we analyzed the lists from Zhao et al. (2016) and Mashonkina et al. (2017). We were guided by the
following criteria:

\begin{enumerate}
	\item The Ba~II 4554\,\AA\ line should not be very strong to avoid the possible influence of the
chromospheric temperature rise in the stellar atmosphere, but it should remain sensitive to a variation in $f_{\rm odd}$. The latter implies that when changing $f_{\rm odd}$ from 0.18 (a solar mixture of isotopes) to 0.46 (a pure $r$-process), the abundance from this line should change at least by 0.1~dex.
\item Both subordinate lines should be reliably measured in the spectrum.
\item The accuracy of log~$g$ is no less than 0.05~dex.
\end{enumerate}

For various reasons, none of the stars in the list of Zhao et al. (2016) was chosen. For example, for
HD~140283 an increase in $f_{\rm odd}$ from 0.18 to 0.46 leads to a decrease in the abundance from Ba~II 4554\,\AA\ by only 0.02~dex, which is less than the error in the total abundance from the subordinate lines.

From the list of Mashonkina et al. (2017) we chose four stars satisfying all criteria (Table~1). The
Ba~II 4554\,\AA\  line in these stars has an equivalent width ($W_{obs}$) in the range from 80 to 140~m\AA. The observed spectra and effective temperatures ($T_{\rm eff}$) were taken from the same paper. The values of log~$g$ were calculated using the distances (Bailer-Jones et al. 2018) based on the Gaia parallaxes. The formula
to calculate log~$g$ also includes $T_{\rm eff}$, the stellar mass, the apparent $V$ magnitude, and the bolometric
correction. Since the stars are old ($-2.6 <$ [Fe/H] $\le -2.2$) and giants, their mass is reliably fixed: $M = 0.8 M_\odot$. The $V$ magnitudes were taken from the SIMBAD\footnote{http://simbad.u-strasbg.fr/simbad/} astronomical database. The bolometric corrections were calculated based on the tables from Alonso et al. (1999). The errors of log~$g$ in Table~1 correspond to the errors in the distances.

We determined the iron abundance from Fe~II lines and the microturbulence velocity from the requirement of the same abundance from Fe~I lines with different $W_{obs}$. Our non-LTE calculations for Fe~I-Fe~II were performed by the method developed previously (Mashonkina et al. 2011), which was updated by taking into account the inelastic processes in Fe~I + H~I and Fe~II + H~I collisions with the rate coefficients from
the quantum-mechanical calculations of Yakovleva et al. (2018, 2019).

\section{NON-LTE CALCULATIONS FOR Ba II}\label{Sect:method}

\subsection{The Ba II Model Atom}

In the atmospheres of metal-poor stars the electron number density is low and the inelastic processes in collisions with neutral hydrogen atoms play an important role in establishing the statistical equilibrium
(SE) of atoms. Belyaev and Yakovleva (2018) were the first to derive the rate coefficients from
their quantum-mechanical calculations of Ba~II + H~I collisions. In this paper the non-LTE calculations
for Ba~II were performed with the model atom from Mashonkina et al. (1999), which was updated by
replacing the approximate Drawinian rates of collisions with H I atoms (Drawin 1968; Steenbock and Holweger
1984) with the accurate data from Belyaev and Yakovleva (2018).

\begin{figure*}
\includegraphics[width=80mm]{ba_bb_rates35_ma4600g160m253_nov2017.eps}
\includegraphics[width=80mm]{ba_bf_rates35_ma4600g160m253_nov2017.eps}
\caption{Left panel: Excitation rates, log~C~(СЃ$^{-1}$), for Ba~II transitions in collisions with electrons (triangles) and H~I atoms (red circles, using the data from Belyaev and Yakovleva, 2018). The open circles correspond to the Drawinian rates scaled by a factor of \kH\ = 0.01.
 Right panel: Rates of the processes Ba$^+ + {\rm e^-} \rightarrow {\rm Ba}^{++} + 2 e^-$ and Ba$^{+} + {\rm H} \rightarrow {\rm Ba^{++} + H^-}$ using similar symbols. The calculations were made for $T = 4190$~K, log~$N_{\rm e}$(cm$^{-3}$) = 10.5 and log~$N_{\rm H}$(cm$^{-3}$) = 16.3.}
\label{fig:rates}
\end{figure*}

In Fig 1a we compare the electron and H I impact excitation rates for various transitions. The calculations were made with the temperature $T$ = 4190~K, the electron number density log~$N_e$(cm$^{-3}$) = 10.5, and the H~I number density log $N_{\rm H}$(cm$^{-3}$) = 16.3, which correspond to the Ba~II line formation depth (log~$\tau_{5000} \simeq -0.5$) in the $T_{\rm eff}$ / log~$g$ / [Fe/H] = 4600~K/1.6/$-2.5$ model atmosphere. For comparison, we also provide the Drawinian rates scaled by a factor of \kH\, = 0.01 that was found empirically by Mashonkina et al. (1999). This figure shows that the collisions with H~I atoms play no lesser role in establishing
the SE of Ba~II than do the collisions with electrons, despite the fact that for transitions with close excitation energies ($E_{lu}$) the rates in the calculations of Belyaev and Yakovleva (2018) can differ by several
orders of magnitude: up to 10~dex in the energy range $E_{lu} <$ 1.5~eV important for the SE. For each level in the atom the rate of charge exchange Ba+$^{+} + {\rm H} \rightarrow {\rm Ba^{++} + H^-}$ exceeds the electron impact ionization rates by 4-5 orders of magnitude (Fig.~1b), but this does not exert a great influence on the ionization equilibrium of Ba~III/Ba~II, because Ba~II dominates in the total barium concentration.

\begin{figure*}
\includegraphics[width=80mm]{ba_bf_ma4600g140m260_pure_e.eps}
\includegraphics[width=80mm]{ba_bf_ma4600g140m260_bel2.eps}
\caption{b-factors of selected Ba II levels in the 4600/1.40/$-2.57$ model atmosphere. Left panel: calculations with purely electron collisions. Right panel: calculations include the collisions with H~I atoms using the data from Belyaev and Yakovleva (2018). }
	\label{fig:bf}
\end{figure*}

The system of SE and radiative transfer equations was solved in a given model atmosphere using an updated DETAIL code (Butler and Giddings 1985). Figure~2 shows the b-factors, b = n$_{\rm NLTE}$/n$_{\rm LTE}$, in
the 4600/1.40/$-2.57$ model atmosphere calculated with and without collisions with H~I atoms. Here, n$_{\rm NLTE}$ an n$_{\rm LTE}$ are the non-LTE and the Boltzmann-Saha level populations. As would be
expected, including the collisions with H~I atoms reduces the departures from LTE. Despite the fact
that Ba~II is the dominant ionization stage, in the case of purely electronic collisions, the b-factors of even the ground and lower excited levels differ noticeably from unity in the Ba~II line formation region, log~$\tau_{5000}$ = 0 to $-1$, and the b-factors of the \eu{5d}{2}{D}{}{3/2} and \eu{5d}{2}{D}{}{5/2} fine-splitting sublevels begin to diverge already in deep layers (log~$\tau_{5000} \sim 0$).

\begin{table}
	\caption{Atomic parameters of the investigated Ba~II lines.}
	\label{tab:listba}
\begin{center}
	\begin{tabular}{ccrcrc}\hline\hline \noalign{\smallskip}
		$\lambda$ & $E_{\rm exc}$ & log $gf$ & log$\Gamma_6$ & \multicolumn{2}{c}{Ref.}  \\
		\cline{5-6}
		(\AA)    & (eV)  &    &  & $gf$  & $\Gamma_6$      \\
		\noalign{\smallskip} \hline \noalign{\smallskip}
		Ba~II 4554.03 & 0.00 & 0.17 & $-$7.732 & \cite{Gallagher_ba} & \cite{Mashonkina2006} \\
		Ba~II 5853.67 & 0.60 & $-$1.01 & $-$7.584 & \cite{Gallagher_ba} & \cite{1998MNRAS.300..863B}  \\
		Ba~II 6496.90 & 0.60 & $-$0.38 & $-$7.584 & \cite{Gallagher_ba} & \cite{1998MNRAS.300..863B}  \\
		Eu~II 4129.72 & 0.00 &    0.22 &  $-$7.870 & \cite{Lawler_eu} &  \\
		\noalign{\smallskip}\hline
	\end{tabular}
\end{center}
\end{table}

\subsection{Synthetic-Spectrum Computations}

The barium and europium abundances are determined by the synthetic-spectrum method, i.e., by fitting the theoretical line profile to the observed one. We use the SynthV code (Tsymbal et al. 2019) together with BinMag\footnote{http://www.astro.uu.se/\~{}oleg/binmag.html}. The b-factors needed to compute the theoretical non-LTE spectra are calculated with the DETAIL code. The list of lines, atomic data, and their sources are given in Table~2. The Eu~II 4129\,\AA\ line is insensitive to the pressure effects, and we adopted log~$\Gamma_6 = -7.870$, by analogy with the Fe~II lines.

For a solar mixture of isotopes the Ba~II 4554\,\AA\ resonance line has 15 components. Since the isotopes $^{134}$Ba and $^{136}$Ba are not produced in the $r$-process, the line consists of 13 components. We use the wavelengths and relative intensities of the components as in our previous studies (see Table~1 in Mashonkina and Zhao, 2006). In our calculations for a different mixture of even and odd isotopes, we treat the change in their relative abundance as a change in the oscillator strengths of the components. For Ba~II 5853 and 6497\,\AA\ the HFS effect is very small: our calculations with and without HFS give a difference in abundance of less than 0.01~dex. Therefore, we use the set of components and their atomic parameters from the VALD database
(Ryabchikova et al. 2015) everywhere for these lines.

The model atmospheres were obtained by interpolation for given $T_{\rm eff}$/log~$g$/[Fe/H] in the
MARCS\footnote{\tt http://marcs.astro.uu.se} grid of models (Gustafsson et al. 2008).
The interpolation algorithm from the MARCS site was used.

\subsection{The Influence of Non-LTE on the Barium Abundance Determination}

The effect from the application of the accurate rate coefficients for collisions with H~I was first checked for the solar Ba~II 5853 and 6497\,\AA\ lines. The spectrum of the Sun as a star was taken from the atlas of Kurucz et al. (1984). The MARCS model atmosphere with $T_{\rm eff}$\ = 5777~K and log~$g$ = 4.44 is used. We adopt $\xi_t$ = 0.9~km\,s$^{-1}$. Under the LTE assumption we get $\eps{}$ = 2.34 and 2.39 for Ba~II 5853 and 6497\,\AA, respectively. This is greater than the meteoritic barium abundance, $\eps{met}$ = 2.21$\pm$0.04 (Lodders et al. 2009). The standard abundance scale, in which $\eps{H}$ = 12, is used here. Non-LTE leads to a strengthening of the Ba~II lines and a reduction in the deduced abundance. When only the electronic collisions are taken into account, $\eps{}$ = 2.21 (Ba~II 5853\,\AA) and 2.23 (Ba II 6497\,\AA), which is consistent with $\eps{met}$. Note that we obtained the same results previously (Mashonkina et al. 1999). Allowance for the collisions with H~I causes the departures from LTE to decrease, and we get a slightly higher abundance, $\eps{}$ = 2.25 and 2.26, although the discrepancies with the meteoritic one do not exceed the determination error. The theoretical non-LTE profiles that describe best the solar Ba~II lines are shown in Fig.~3.

\begin{figure*}
\includegraphics[width=80mm]{sun_ba5853.eps}
\includegraphics[width=80mm]{sun_ba6496.eps}
\caption{Ba II lines in the solar spectrum (dotted curves) and the theoretical non-LTE (solid curves) and LTE
(dashed curves) profiles computed with $\eps{}$ = 2.25 and 2.26 for Ba~II 5853 and 6497~\AA, respectively.}\label{fig:solar}
\end{figure*}

We calculated the non-LTE abundance corrections, $\Delta_{\rm NLTE} = \eps{NLTE} - \eps{LTE}$, for five Ba~II
lines, three from Table~2 as well as Ba~II 4934 and 6141\,\AA, and for two grids of model atmospheres. One
of them has a range of parameters typical for cool giants: $T_{\rm eff}$\ = 4500 and 4750~K, log~$g$ from 0.5 to 2.5
with a 0.5 step, and [Fe/H] = 0, $-1$, $-2$, $-2.5$, $-3$. The other one has a range of parameters typical for stars of late spectral types near the main sequence: $T_{\rm eff}$\ from 4500 to 6500~K with a step of 500~K, log~$g$ from 3.0 to 4.5 with a 0.5 step, and [Fe/H] from 0 to $-3$ with a $-0.5$ step. The tables of corrections
are accessible at {\tt http://www.inasan.rssi.ru/$\sim$lima/NLTE\_corrections/}.

The non-LTE corrections for three lines at two values of $T_{\rm eff}$\ are presented in Fig.~4. As was first
shown by Mashonkina et al. (1999), the departures from LTE for Ba~II lines can have different signs and
values, depending on the stellar metallicity, $T_{\rm eff}$, and log~$g$. The picture does not change qualitatively in the calculations with more accurate collisional data either, as can be seen from Fig.~4. At a solar metallicity non-LTE leads to a strengthening of the Ba~II lines and a negative $\Delta_{\rm NLTE}$, irrespective of $T_{\rm eff}$\ and log~$g$. We note that the non-LTE effects are small for Ba~II 4554\,\AA\ in cool giants in a wide
metallicity range, because this line is very strong, with well-developed van der Waals wings forming in
deep atmospheric layers. In models with log~$g \ge 3$, the non-LTE effects grow, i.e., $\Delta_{\rm NLTE}$ becomes more negative, as [Fe/H] decreases to a certain value that depends on the line, log~$g$, and $T_{\rm eff}$. As [Fe/H] decreases further, the non-LTE corrections are reduced in absolute value, pass through 0, and become
positive. This is because the lines weaken and their formation depths are shifted into deep atmospheric
layers. When the Ba~II line is strong, the non-LTE effect takes place in its core and it is attributable to
dropping the line source function relative to the Planck function in the surface layers due to the escape of photons in the line itself, which leads to a depopulation of the upper level relative to the lower one. When the Ba~II line is weak, it is formed in deep layers, where the upper levels are overpopulated relative to the lower ones, which leads to a line weakening compared to the LTE case.

\begin{figure*}
	\hspace{-6mm}
\includegraphics[width=50mm]{ba4554_dnlte.eps}
\includegraphics[width=50mm]{ba5853_dnlte.eps}
\includegraphics[width=50mm]{ba6497_dnlte.eps}
\caption{Non-LTE abundance corrections for the Ba~II 4554,  5853 and 6497~\AA\ lines as a function of
metallicity and surface gravity. log\,$g$ takes values of 3.0, 3.5, 4.0, 4.5 in the models with $T_{\rm eff}$\ = 6000~K and 0.5, 1.0, 2.0, 3.0 in the models with $T_{\rm eff}$\ = 4500~K. The non-LTE corrections are not shown if the line equivalent width falls below 3~m\AA. }\label{fig:dnlte}
\end{figure*}

\section{THE BARIUM AND EUROPIUM ABUNDANCES OF THE PROGRAM STARS}\label{Sect:Abund}

The Ba~II lines in the spectra of the program stars are shown in Fig.~5. The procedure for matching the
observed and theoretical profiles leads to an uncertainty in the abundance of no more than 0.02~dex. For
Ba~II 4554\,\AA\ the calculations were carried out with  $f_{\rm odd}$ = 0.18, 0.30, 0.35, and 0.46. The results of our LTE and non-LTE abundance determinations are presented in Table~3, except the abundance for $f_{\rm odd}$ = 0.35.

\begin{table*}
	\caption{LTE and non-LTE abundances from the Ba~II lines at a given fraction of odd isotopes ($f_{\rm odd}$). The uncertainties in the abundance due to the uncertainty in the atmospheric parameters are given for each line.}
	\label{tab:lines}
\begin{center}
	\begin{tabular}{lccccc}\hline\hline \noalign{\smallskip}
$\lambda$, \AA & 5853 & 6496 & \multicolumn{3}{c}{4554} \\
 \cline{4-6}
$f_{\rm odd}$ & 0.46 &  0.46 & 0.18 & 0.30 & 0.46  \\
\hline\hline
\multicolumn{6}{c}{HD 2796}  \\
$\eps{}$, LTE &  -0.42 &  -0.25 &  -0.08 &  -0.21 &  -0.32  \\
\cline{2-3}
Mean & \multicolumn{2}{c}{$-0.34\pm0.12$} & & & \\
$\Delta_{\rm NLTE}$ &   0.02 &  -0.11 &  -0.09 &  -0.09 &  -0.10 \\
 $\eps{}$, non-LTE &  -0.40 &  -0.36 &  -0.17 &  -0.30 &  -0.42  \\
\cline{2-3}
Mean  & \multicolumn{2}{c}{$-0.38\pm0.03$} & & & \\
\multicolumn{6}{c}{Uncertainties in abundance (dex)} \\
$T_{\rm eff}$, 100~K &   0.06 &   0.07 &   0.10 &   0.10 &   0.10  \\
log\,$g$, $-0.05$ & -0.02 &  -0.02 &  -0.01 &  -0.01 &  -0.01  \\
$\xi_t$, 0.1~km\,s$^{-1}$ & -0.01 &  -0.05 &  -0.09 &  -0.09 &  -0.09 \\
\hline\hline
 \multicolumn{6}{c}{HD 108317} \\
$\eps{}$, LTE &   -0.05 &   0.01 &   0.39 &   0.27 &   0.17 \\
\cline{2-3}
Mean &  \multicolumn{2}{c}{$-0.02\pm0.04$} & & & \\
$\Delta_{\rm NLTE}$ &   0.02 &  -0.08 &  -0.14 &  -0.15 &  -0.17 \\
$\eps{}$, non-LTE &  -0.03 &  -0.07 &   0.25 &   0.12 &   0.00 \\
\cline{2-3}
Mean  & \multicolumn{2}{c}{$-0.05\pm0.03$} & & & \\
\multicolumn{6}{c}{Uncertainties in abundance (dex)} \\
$T_{\rm eff}$, 100~K &  0.06 &   0.07 &   0.11 &   0.11 &   0.11 \\
log\,$g$, $-0.03$ &  -0.01 &  -0.01 &   0.00 &   0.00 &   0.00 \\
$\xi_t$, 0.1~km\,s$^{-1}$ &  -0.01 &  -0.04 &  -0.07 &  -0.07 &  -0.07 \\
\hline\hline
\multicolumn{6}{c}{HD 122563} \\
$\eps{}$, LTE &  -1.45 &  -1.36 &  -1.22 &  -1.33 &  -1.44   \\
\cline{2-3}
Mean & \multicolumn{2}{c}{$-1.40\pm0.06$} & & &  \\
$\Delta_{\rm NLTE}$ & 0.07 &   0.03 &   0.04 &   0.04 &   0.04 \\
 $\eps{}$, non-LTE &  -1.38 &  -1.33 &  -1.18 &  -1.29 &  -1.40  \\
\cline{2-3}
Mean & \multicolumn{2}{c}{$-1.36\pm0.04$} & & & \\
\multicolumn{6}{c}{Uncertainties in abundance (dex)} \\
$T_{\rm eff}$, 50~K &   0.05 &   0.05 &   0.05 &   0.05 &   0.05  \\
log\,$g$, $-0.03$ &  -0.02 &  -0.01 &  -0.01 &  -0.01 &  -0.01 \\
$\xi_t$, 0.1~km\,s$^{-1}$ &  -0.00 &  -0.02 &  -0.06 &  -0.06 &  -0.06  \\
\hline\hline
\multicolumn{6}{c}{HD 128279} \\
$\eps{}$, LTE &  -0.49 &  -0.43 &  -0.25 &  -0.39 &  -0.51 \\
\cline{2-3}
Mean & \multicolumn{2}{c}{$-0.46\pm0.04$} & & & \\
$\Delta_{\rm NLTE}$ &  0.04 &  -0.01 &  -0.08 &  -0.07 &  -0.06 \\
$\eps{}$, non-LTE &  -0.45 &  -0.44 &  -0.33 &  -0.46 &  -0.57 \\
\cline{2-3}
Mean &  \multicolumn{2}{c}{$-0.45\pm0.01$} & & & \\
\multicolumn{6}{c}{Uncertainties in abundance (dex)} \\
$T_{\rm eff}$, 100~K &   0.06 &   0.06 &   0.10 &   0.10 &   0.10 \\
log\,$g$, $-0.03$ &  -0.00 &   0.01 &  -0.01 &  -0.01 &  -0.01 \\
$\xi_t$, 0.1~km\,s$^{-1}$ &  -0.00 &  -0.02 &  -0.05 &  -0.05 &  -0.05 \\
\hline
\end{tabular}
\end{center}
\end{table*}

\begin{figure*}
\includegraphics{hd2796_ba3_diff.eps}
\includegraphics{hd108317_ba3_diff.eps}
\includegraphics{hd122563_ba3_diff.eps}
\includegraphics{hd128279_ba3_diff.eps}
	\caption{Ba II lines in the stellar spectra (dotted curves) and the theoretical non-LTE spectra (solid curves) computed with the abundances from Table~3. The calculations of Ba~II 4554~\AA\ were made with $f_{\rm odd}$ = 0.18 (lilac dotted curves), 0.46 (blue dashed curves), and the value derived for a given star (red solid curves), as indicated in Table~4. The corresponding O-C values are shown in the upper part of each panel for Ba~II 4554~\AA. }\label{fig:lines}
\end{figure*}

For the star HD 122563 with the lowest metal abundance in our sample non-LTE leads to a weakening of all three Ba~II lines and positive abundance corrections (Table~3). In the remaining three stars, $\Delta_{\rm NLTE} > 0$ only for the weakest line, Ba~II 5853~\AA, while for the other two lines non-LTE leads to their strengthening and $\Delta_{\rm NLTE} < 0$.

For each star the difference in the abundance deduced from the two subordinate lines is smaller in the non-LTE calculations than in the LTE ones. We estimate the accuracy of determined total barium abundance by the root-mean-square error, $\sigma = \sqrt{\Sigma(\overline{x}-x_i)^2/(n-1)}$, where $n$ = 2 is the number of subordinate lines. In the non-LTE calculations, $\sigma$ does not exceed 0.04~dex.

The HFS components formed by the isotopes $^{135}$Ba and $^{137}$Ba increase the full width at half maximum (FWHM) of the Ba~II 4554~\AA\ line. An increase in $f_{\rm odd}$ leads to a growth in the FWHM and absorption and a reduction in the abundance from this line. For the program stars the difference in abundance between $f_{\rm odd}$ = 0.18 and 0.46 is between 0.22 and 0.25~dex. This is considerably larger than the error in the total barium abundance, which makes it possible to determine $f_{\rm odd}$ from the requirement that the abundances from the resonance and subordinate lines be equal.

To compare two indicators of $r/s$, $f_{\rm odd}$ and [Eu/Ba], the abundance was also determined for europium. The non-LTE calculations were performed with the model atom from Mashonkina et al. (2000). Due to the absence of accurate data for collisions with H I, we use the Drawinian rates scaled by a factor of \kH\ = 0.1. Non-LTE leads to a weakening of the Eu~II 4129~\AA\ line and a higher europium abundance, by 0.07-0.1~dex
for different stars. Europium is represented in nature mainly by two isotopes, $^{151}$Eu and $^{153}$Eu, and each of them forms 16 HFS components in the Eu~II 4129~\AA\ line. The $s$-process calculations and the "solar" $r$-process based on them predict that the relative yield of
europium isotopes is similar in the  $s$- and $r$-processes (see, e.g., Travaglio et al. 1999; Bisterzo et al. 2014) and close to the solar abundance ratio: $^{151}$Eu : $^{153}$Eu = 47.8 : 52.2 (Lodders et al. 2009). The set of Eu~II 4129~\AA\ line components and their $gf$-values corresponding to a solar mixture of isotopes were taken from the VALD database. The results of our abundance determinations are presented in Table~4.

\begin{table*}
	\caption{Non-LTE barium and europium abundances and the fraction (in \%) of odd barium isotopes}\label{tab:abund}
\begin{center}
	\begin{tabular}{rccccc}
		\hline\hline
\multicolumn{1}{l}{HD}  & [Fe/H] & $\eps{Ba}$     & $\eps{Eu}$ & [Eu/Ba] & $f_{\rm odd} \times$ 100 \\
\hline
		2796   &  $-2.19$ & $-0.38\pm0.03$ & $-1.73$ & 0.31 & 40$^{51}_{29}\pm 5$  \\
		108317 &  $-2.24$ & $-0.05\pm0.03$ & $-1.11$ & 0.60 & 53$^{61}_{45}\pm 4$ \\
		122563 &  $-2.55$ & $-1.35\pm0.04$ & $-2.70$ & 0.31 & 39$^{45}_{33}\pm 6$ \\
		128279 &  $-2.19$ & $-0.43\pm0.03$ & $-1.65$ & 0.44 & 27$^{35}_{21}\pm 1$  \\
\hline
\end{tabular}
\end{center}
\end{table*}

{\bf Uncertainties in the derived barium abundances.} We analyzed the influence of uncertainties in the atmospheric parameters on the abundance deduced from the resonance and subordinate lines. The errors in the effective temperature were taken from the original sources. The errors in log~$g$ were calculated by taking into account the distance errors, as given by Bailer-Jones et al. (2018). We estimate the microturbulence error as 0.1~km\,s$^{-1}$. The results are presented in Table~3. The influence of the error in log~$g$ on the abundance is virtually the same for different lines and it is small. The Ba~II 4554\,\AA\ line with $W_{obs}$ in the range from 80 to 140~m\AA\ lies on the saturation part of the curve of growth and, therefore, it is more sensitive to the errors in $T_{\rm eff}$\ and $\xi_t$ than the subordinate lines. Note that for an individual star the abundance errors due to the uncertainty in a given atmospheric parameter are not statistical, but systematic in nature for different lines. For example, for HD~2796 an error of 100~K in $T_{\rm eff}$\ leads to a difference of 0.04~dex in abundance between the resonance and subordinate lines, while an error of 0.1~km\,s$^{-1}$\ in $\xi_t$ leads to a difference of 0.06~dex in abundance. Since the errors in $T_{\rm eff}$\ and $\xi_t$ are uncorrelated, the total abundance error due to the errors in the atmospheric parameters will be $\sigma_{atm}$ = 0.07~dex.

The uncertainty in the data for Ba~II + H~I collisions can also be a source of errors in the abundance. An upper limit for this error can be estimated by comparing the abundances deduced in the non-LTE calculations with and without collisions with H~I. This error is also systematic in nature, because ignoring the collisions with H~I leads to an enhancement of the departures from LTE for both resonance and subordinate lines, but to a different extent. For example, for HD~122563 allowance for only the electronic collisions leads to an increase in
the abundance compared to what is obtained when the collisions with H~I are taken into account, by 0.07~dex from Ba~II 4554\,\AA\ and by 0.06~dex and 0.02~dex from Ba II 5853 and 6497\,\AA. In other stars, the shift in the abundance from the Ba~II 4554, 5853, and 6497\,\AA\ lines is: +0.05,+0.05, and +0.05 dex (HD~2796); +0.05,+0.02, and $-0.01$~dex (HD~108317); and +0.02,+0.03, and +0.02 dex (HD~128279).

\section{DETERMINATION OF $f_{\rm odd}$ AND DISCUSSION OF RESULTS}
\label{sect:fodd}

For each star $f_{\rm odd}$ was derived from the requirement that the abundances determined from the resonance
and subordinate lines be equal. The values of $f_{\rm odd}$ are given in Table~4. The statistical error in $f_{\rm odd}$ is determined by the error in the total barium abundance ($\sigma$). We also provide the upper and lower
limits for $f_{\rm odd}$ estimated by taking into account the errors in the atmospheric parameters ($\sigma_{atm}$). Let us give an example for the star HD~2796. We obtained $\eps{NLTE} = -0.38$ from the subordinate lines, while Ba~II 4554\,\AA\ gives $\eps{NLTE} = -0.35$ and $-0.42$ at $f_{\rm odd}$ = 0.35 and 0.46. By assuming that
in this interval $\eps{}$ depends linearly on $f_{\rm odd}$, we get $f_{\rm odd}$ = 0.40. Since $\sigma$ = 0.03~dex, the statistical error in $f_{\rm odd}$ is $\pm 0.05$. The errors in the atmospheric parameters give $\sigma_{atm}$ = 0.07~dex. A shift in the total barium abundance by $+-0.07$~dex implies a change in $f_{\rm odd}$ by $-+0.11$ for HD~2796.

Changing the line formation scenario or, more specifically, passing to allowance for the collisions only with electrons does not affect the determination of $f_{\rm odd}$ for HD~2796 and HD~128279, because this shifts the abundances from the resonance and subordinate lines by the same amount. For the other two stars the abundance from the resonance line increases by a larger value than the one from the subordinate lines. For each of them this implies that $f_{\rm odd}$ can be larger than its value in Table~4, by 0.05.

For three stars we obtained $f_{\rm odd} \ge$ 0.4. This points to a significant or even dominant contribution of
the $r$-process to the observed barium abundances. For the $r$-process Travaglio et al. (1999), Kratz et al. (2007), and Bisterzo et al. (2014) predicted $f_{\rm odd,r}$ = 0.46, 0.44, and 0.60, respectively. If we adopt $f_{\rm odd,r}$ = 0.46, then $f_{\rm odd}$ = 0.4 observed in the star implies that 83~\%\ of its barium was produced in
the $r$-process. The dominance of the $r$-process at the formation epoch of our objects is independently confirmed by the observed europium overabundance relative to barium, with [Eu/Ba] $> 0.3$. The same authors predicted [Eu/Ba]$_r$ = 0.67, 0.63, and 0.80 for the $r$-process. We note the large scatter of predicted values and the agreement of the observations only with the lower boundary of the predictions. In HD~128279, $f_{\rm odd}$ = 0.27 exceeds the solar value, though insignificantly, while [Eu/Ba] = 0.44 suggests a substantial contribution of the $r$-process to the barium abundance.

Of the four stars, $f_{\rm odd}$ was determined previously only for HD~122563, but a lower value of 0.22$\pm$0.15 was obtained by Mashonkina et al. (2008). The previous paper differs from this one in that other
values of log~$g$ = 1.5 and $\xi_t$ = 1.9~km\,s$^{-1}$\ were used and that the collisions with H~I were disregarded. Our analysis showed that the difference in $\xi_t$ is mainly responsible for the difference in $f_{\rm odd}$. Mashonkina et al. (2008) obtained a higher microturbulence velocity, because they used only Fe~II lines, which have a limited range of equivalent widths in a star with [Fe/H] $\simeq -2.5$, while an efficient non-LTE method
has not yet been developed for Fe~I lines. Thus, we confirm that the method of determining $f_{\rm odd}$ used in
our paper is very sensitive to the accuracy of determining the atmospheric parameters, including $\xi_t$.

Among several works on the determination of $f_{\rm odd}$ by a method that differs from our one and is based on
the dependence of the FWHM of the Ba~II 4554\,\AA\ line on the abundance of odd isotopes, we will allude
only to Gallagher et al. (2015), where the line profile was computed in a 3D model atmosphere. For the
halo star HD~140283 ([Fe/H] $\simeq -2.4$) they obtained $f_{\rm odd}$ = 0.38$\pm$0.02 with a systematic error of 0.06.

We checked how using accurate rate coefficients for the collisions with H~I affects the determination of $f_{\rm odd}$ for two stars in the Sculptor dwarf spheroidal galaxy, ET0381 and 03\_059. Jablonka et al. (2015) used the same method as that in this paper, except for the non-LTE calculations in which the collisions with
H~I were taken into account with the Drawinian rates reduced by a factor of 100, and obtained $f_{\rm odd} \le$ 0.11. Such low values point to the dominance of the $s$-process at the epoch when the stars were formed. However, this is a very strange result, because both stars are metal-poor, with [Fe/H] = $-2.19$ and $-2.88$, and they are expected to have been formed before the first AGB stars appeared in the dwarf galaxy and nucleosynthesis in the $s$-process began. Jablonka et al. (2015) convincingly proved that the existing uncertainties in the atmospheric parameters could not be responsible for the low $f_{\rm odd}$. Later on, the atmospheric parameters of both stars were carefully double checked (Mashonkina et al. 2017). The non-LTE calculations with accurate rate coefficients for Ba~II + H~I collisions confirmed the previously published $f_{\rm odd}$ for the stars ET0381 and 03\_059. For the first star the abundance from the subordinate lines decreased by 0.015~dex and the one from the Ba~II 4554\,\AA\ line did not change. For the second star new calculations led to the same decrease in the abundance from all Ba~II lines, by 0.03~dex. The [Eu/Ba] ratios cannot be determined in these stars, because it is impossible to measure the Eu~II lines. Thus, the question about the source of barium in the Sculptor dwarf spheroidal galaxy at the formation epoch of very metal-poor stars remains unsolved.

\section{CONCLUSIONS}\label{sect:conclusions}

The Ba~II model atom developed previously (Mashonkina et al. 1999) was updated by taking into account the H~I impact excitation and using the rate coefficients from the quantum-mechanical calculations of Belyaev and
Yakovleva (2018). As expected, the non-LTE calculations with this model atom lead to a reduction in the
departures from LTE compared to the case where the collisions only with electrons are taken into account.
With the new model atom we calculated the non-LTE abundance corrections for five Ba~II lines and investigated
their dependence on atmospheric parameters in the ranges $T_{\rm eff}$\ = 4500-6500~K, log~$g$ = 0.5-4.5, and [Fe/H] from 0 to $-3$. The tables of corrections are accessible at {\tt http://www.inasan.rssi.ru/$\sim$lima/NLTE\_corrections/}.

To determine the fraction of barium isotopes with an odd mass number, we chose four Galactic halo giants for which there are high-resolution and high S/N spectra and reliable atmospheric parameters, namely the effective temperature and surface gravity, obtained from non-spectroscopic methods based, among other things, on the Gaia
parallaxes (Gaia Collaboration 2018). We used a method based on the requirement that the abundances from the Ba~II 4554\,\AA\ resonance line and the Ba~II 5853 and 6497\,\AA\ subordinate lines be equal. A combination of accurate atmospheric parameters, high-quality observed spectra, and theoretical spectra computed with the most complete accounting for the physical processes in the Ba~II atom provides a high accuracy of determining the abundance from individual lines. Good agreement between the non-LTE abundances from the two subordinate lines, so that for each star the standard deviation does not exceed 0.04~dex, serves as a confirmation.

For three stars (HD~2796, HD~108317, and HD~122563) $f_{\rm odd} \ge$ 0.4. This suggests that $\ge$80~\%\ of the barium observed in these stars was synthesized in the $r$-process. Our estimate was obtained using $f_{\rm odd,r}$ = 0.46 (Travaglio et al. 1999). In HD~128279, our value of $f_{\rm odd}$ = 0.27 exceeds the fraction of odd
isotopes in the Solar system, but only slightly. The dominance of the $r$-process at the formation epoch of
our sample stars is confirmed by the presence of a europium overabundance relative to barium, with [Eu/Ba] $> 0.3$.

{\it Acknowledgements.} We are grateful to Rana Ezzeddine who provided the spectra of HD~108317. We used the
VLT2/UVES archive of observed spectra and the ADS\footnote{http://adsabs.harvard.edu/abstract\_service.html}, SIMBAD, MARCS, and VALD databases. The work presented in Section~2 was performed as part of RSF project no. 17-13-01144.

redpajama_set_name: RedPajamaArXiv


The link, just in case: I am Rizen.
I appreciate your feedback, constructive criticism and time!
Has anyone given it a listen?
I would really appreciate some feedback!
i lissened the first 15 minutes while surfing the interenet, so not that.......attentively ??
But it sounds Verry good to me!
I listened to your mix while working out and watching NASCAR's Pure Michigan 400. Really! Here's my feedback.
- Thanks for the tracklisting! And good info in post title/message body! I like download links too, but this helps!
- Intro track seems appropriate, you are throwing down the gauntlet and declaring this will be a progressive mix. Second track is a nice intro, brings the energy to around a 7 or so.
- Slight volume bobble on the mix into the third track (~3:45?) but nice transition/mix imo.
- 7:15 and so far this mix is pretty kickin. Some more volume issues around here with your overall track levels.
- 9:30 and I'm glad to hear the (florence) vocal. Was getting a bit blippity bloopity for me. I'm also getting a bit overwhelmed by the numbers of breakdowns and builds, but I understand that's part of the genre of music you play.
- The mix out of that florence track (~13:00) was a little rough for me. Harmonically? In terms of EQ? Something.
- At about 20:00, I'm reminded why I really don't prefer progressive house by a weirdly emo euro vocal. But you have settled into a nice prog house groove and I can't complain too much. I like the phrasing of the mix right around here.
- 21:30, another breakdown and build. progressive house, I remind myself, and don't blame you.
- Jimmie Johnson, ol' Five Time, seems to be running away with this race.
- Nice, a little bit of a groove without an immediate breakdown or build. 28 minutes, a vocal. alright.
- There seem to be relatively serious changes in volume throughout your mix, especially when you are in the mix. I appreciate the attention to detail in terms of subtle fading, but it seems like you might be EQing and/or changing the levels a little "too much".
- ~36:00 I feel like the phrasing is off by a measure, you mix in a measure too soon.
- NASCAR SPOILERS : Damn, Kyle Busch pulls it out after a G-W-C finish.
- I eventually finish my workout and turn off your mix around an hour. All progressived-out.
Brotha, I just want to say that you rock, and I really appreciate you stepping out of your musical norm to listen to my mix.
As far as that transition from the "florence track" into the next: I could never quite figure out what was odd about it, but I'm glad that you pointed it out. I think that it could be a minor/major chord thing (?).
Anyways, I really appreciate your response, and your feedback with detail!


With three weeks to go until Derby Day ticket sales for the clash between Saracens and Harlequins on the 16th April have hit 65,000.
Group deals in particular for the game have been soaring with local rugby clubs eager to be part of a special day out at Wembley Stadium. Local Club Billericay RFC have a group of over 350 attending the game while Ely Tigers are bringing 239 along with them and Luton RFC have a group of 200 heading to the National Stadium for the game.
With 11 of England's Six Nations winning squad due to be in action on the day the game is shaping up to be one of the highlights of the season for rugby fans across the capital.
Saracens will also be joined by pop star Foxes who will be entertaining the crowd ahead of the game with her some of the biggest hits from her recent album.
Tickets are available for the fixture from just £7.50 for juniors so why not join the rest of the Sarries family at Wembley this April?


Governor Ibikunle Amosun of Ogun State, on Sunday, declared that despite the clearance given by the National Working Committee (NWC) to Dapo Abiodun as the governorship candidate of the All Progressives Congress (APC) in the state, his anointed candidate, Hon. Abdul-Kabir Adekunle Akinlade, will succeed him in 2019.
He insisted that as far as he and other party members in the state were concerned, Akinlade would emerge as the next governor of the state.
"They have told Mr. President all manners of stories, that Amosun has done this or that. Amosun will stand for justice, fairness and the truth.
"That is why in Ogun State come May 29, 2019, to the glory of God and the benevolence of Almighty God, Hon. Adekunle Akinlade will be the governor of the state.


From the artistic vision of Dominic V. Duong, comes DVDance's second season, Convergence. An evening of dance celebrating the directors 'hopes, dreams, and wishes' of uniting artists and presenting them on stage.
Season Two introduces company choreographer, Ryan Kwok and joining the stage is Sangam Art's - Navia Natarajan, presenting a modern Indian dance solo. Danny Tran dances a contemporary ballet solo; courtesy of The Los Gatos Ballet. From Santa Barbara, Ca., Tracy Kofford will present "Intersecting Fugue", and from NYC's Broadway Dance Center, Rickey Tripp joins the production as a guest choreographer. DVDance is also proud to present the International Performing Arts of America on our program.


The Lagoon menu is available for take-away 7 days a week from 5pm. When selecting a time to pick-up your order, please allow minimum 45 minutes for us to freshly prepare your order.
Takeaway Seafood Platter for Two, only $150 The Lagoon is offering a special seafood platter to lovers and lovers of seafood this Valentine's Day. Order ahead and then take away a mouthwatering selection of top-grade local seafood cooked by award-winning haute chefs—and enjoy your meal in whatever secluded getaway means the most to you. HOT & COLD SEAFOOD PLATTER FOR TWO Hot: Whole lobster mornay, Moreton Bay buys, BBQ king prawns, Kilpatrick and mornay oysters, scallops in the shell, BBQ octopus, salt & pepper calamari, and catch of the day Cold: Balmain bugs, blue swimmer crab, natural oysters, fresh king prawns, yellow in tuna, and beetroot-cured Atlantic salmon Order any time until 5pm 14 Feb and pick up on the day between 5pm and 7pm.


Villa Bougainvillaea is one of three villas (the other two are called Gardenia and Jasmine) on a hillside overlooking the west coast, just outside the tiny hamlet of Vlachoplatika. Bougainvillaea is the middle villa.
The hillside and the surrounding valleys are beautifully natural: terraces of olive groves, dry stone walls, pine forest and cypress copse.
The positioning of each villa is staggered and bordered by tall pine trees for privacy.
This is a peaceful and secluded part of the island and the views out to sea are dramatic.
Location: car hire recommended. The village of Bogdanatika, just under a kilometre away, has 2 tavernas and a supermarket. Magazia, about a kilometre away, has 2 tavernas, 2 café bars and a minimarket. It is a 10 minute drive to the shops, tavernas, boat hire and beaches of Loggos, Lakka or Gaios, and a 10 minute drive to Erimitis beach.
Open-plan sitting room, dining area and kitchen; one double bedroom; bathroom with shower.


text:
Bomb scare delays Hudson parade
Bill Shaner Daily News staff @bill_shaner
Nov 11, 2016 at 12:18 PM Nov 11, 2016 at 12:19 PM
HUDSON – A bomb scare delayed and altered the town's annual Veteran's Day Parade Friday morning.
A caller said a suspicious package was outside the Hudson Town Library as the parade prepared for launch, around 10 a.m., prompted organizers to move the start to Town Hall as the State Police Bomb Squad descended. The pivot delayed the parade about 20 minutes.
In the end, the scare was a false alarm. State Police found the threat was a harmless package left at the library door. The library, like all town institutions, was closed today.
"Because of what we were having here today, the Veterans Day Parade, we wanted to err on the side of caution to make sure it wasn't anything suspicious," said Michael Burks, police chief.
Though it was delayed, and the route shortened, organizers said the parade was still a success.
"It was a nice crowd, very good turnout," said Brian Stearns, veteran services director.
He thanked the Police and Fire Departments for a quick response.
"They were unbelievable," said Stearns. "We're very fortunate to have the police and fire we have here."
The Hudson Veterans Day Parade is a roughly 75-year tradition, and one important to the history and culture of the town, said Stearns.
"Without a Veterans Day Parade, traditions are lost," he said.
Bill Shaner can be reached at 508-626-3957 or at wshaner@wickedlocal.com. Follow him on Twitter @Bill_Shaner.

redpajama_set_name: RedPajamaCommonCrawl


I met Anthony Bourdain on October 25, 2008. He was in the Philippines about to film an episode on Filipino food for his TV series, No Reservations. His arrival in the country was unannounced but then word got out and the public relations agency handling his TV network had no choice but to hold an impromptu press conference for the media. It was to be an intimate dinner in Sofitel Philippine Plaza with only a limited number of invitees. I was one of five media personalities privileged to meet him that day.
I confess this today: I only had a vague notion of who Anthony Bourdain was then. Blasphemous, I know. I was only aware of his status as a prominent voice in the culinary scene but I never read any of his books nor watched any of his programs. I knew he was considered a rock star in the food world and he had a cult following. But I was not one of them.
On the day of the press event, Tony walked in the room like a normal person. No mob ensued on the way to the private conference room and he was cordial as he said hello to all of us. At first, it was hard to see the tough persona he was known for but over the course of the dinner, his natural voice emerged and I was a firsthand witness to the wit and humor that has enamored many. He talked about the places he planned to visit in Manila and narrated some of the unforgettable experiences he had filming his show.
I wonder what was going through his head then. Stupid reporter, most probably. Whatever it was, I was not concerned of what he thought then. The interview ended with the obligatory picture taking session and I left, still not a fan.
Over the years since that meeting, I had chanced upon his show and watched it. I have also watched his numerous guestings in shows like Top Chef. I came to admire him, not because of the wide world he opened up to me or the dining destinations he piqued my interest in or the culinary knowledge he imparted to me. Instead, he won me over with his authentic personality and the way he looked at the world. The places he had been to and the food he had eaten, you can see them in any other food and travel show. But nowhere will you see Tony's brand of storytelling delivered with punchlines that would make anyone snicker with glee; or his signature brash attitude and honesty that made you wish you had the same courage to say some things out loud. It was his unflinching attitude towards life that I loved so much. Which is why it is so hard to make sense of the life he has given up today.
I had promised myself that I would make it up to him for asking that unspeakable question. Somehow, I was sure I will meet him again. I will be able to redeem myself in Tony's eyes as the writer who asked that stupid question. Of course, he will not remember me nor the question I asked the day I met him. It was more for myself. I needed this culinary idol to see me in a new light. Over the years, I have accumulated a list of questions in my head to ask him on that fateful day of our reunion. I assure you, they will all be good ones. I'd like to ask why that food mecca he was planning to put up in New York never pushed through or how we can do better to fight food waste, a topic he was passionate about. But most of all, I'd like to ask him how you get over a failed restaurant, something I never seemed to be able to recover from even after many years have passed. Sadly, I will never get the chance to ask him these questions anymore.
There is always this question that comes up when you are around foodies and the topic lingers to Anthony Bourdain: "Where will you bring Anthony Bourdain to eat if he comes back to Manila?" Everyone has their own idea of where to bring him. Then my turn would come and I will always decline to share my answer. People would press me for an answer as if my answer weighed more than others simply because I had met him once in my life. But I never gave in. No one to this day has ever succeeded in prying that answer from me. I have guarded my answer zealously because I firmly believed that one day I will see him again and bring him to that place. No one was going to steal my idea. I know now that I will never get to bring him to the place I want to share with him. I will never ever get redeemed in his eyes. But perhaps by writing this now, I will be able to.
So where will I bring Tony?
It is not a top secret place as everyone thinks it to be. I am amazed that no one has even thought about it after hearing all the myriad places people want to bring him to. We see it everywhere now but in my mind, I know just what to say to pique Tony's interest.
I will tell him of the white halo-halo that comes from a part of our country. Of how this halo-halo was an edited version of the dessert he loves and how the pared-down ingredients worked so harmoniously well with each other.
I imagine his eyes brightening up with curiosity and his excitement in trying it. His love for our halo-halo has always been well publicized and he will surely enjoy a visit to the ubiquitous Razon's we all know. But, unfortunately, I know precisely how that day will turn out.
Tony will kindly say that he likes the halo-halo in Razon's but he still prefers the traditional halo-halo because it won't be what it is if it did not have all those colorful ingredients thrown together. I will offer no objections and keep silent. I will nod and smile in respect to the man I have come to admire. And by then, I would have noticed his empty halo-halo cup and be pleased. Yes, redemption is sweet, but now it's all just wishful thinking.


Detailing the physical features, habits, territorial reach and other identifying qualities of the Black-and-White Click Beetle.
Native to the arid regions of the U.S. Southwest and Mexico, the Black-and-White Click Beetle is found where pockets of moisture spring up.
Long and slender, the Black-and-White Click Beetle has a large, black pronotum ('shoulder' area) that is edged in a creamy white color. The abdomen is also edged in white to varying degrees based on the individual. Some have more white on them than others. When knocked over or placed onto its back, this beetle, like all Click Beetles, can flip itself upright and onto its feet. It is more flexible in the thoracic region than other beetles, allowing it to snap a small spine which then launches the beetle upward. The flip can sometimes reach heights greater than 12 cm (5 inches). The snapping of the spine also creates an audible click.
Black-and-White Click Beetles feed on vegetation that grows in the rare moist areas in desert-like regions in its range. Look for them near willow, Ponderosa pine, oak, and other trees found in the Sonoran desert and southern parts of the Mojave desert.


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HTML and the World Wide Web
1.3 HTML: What It Is
HTML is a document-layout and hyperlink-specification language. It defines the syntax and placement of special, embedded directions that aren't displayed by the browser, but tell it how to display the contents of the document, including text, images, and other support media. The language also tells you how to make a document interactive through special hypertext links, which connect your document with other documents--on either your computer or someone else's, as well as with other Internet resources, like FTP and Gopher.
HTML Standards and Extensions
The basic syntax and semantics of HTML are defined in the HTML standard, currently Version 3.2. HTML is a young language, barely five years old, but already in its third iteration. Don't be too surprised if another version appears before you finish reading this book. Given the pace of these standards matters, one never knows when or if a new standard version will come to fruition.
Browser developers rely upon the HTML standard to program the software that formats and displays common HTML documents. Authors use the standard to make sure they are writing effective, correct HTML documents. Nonetheless, commercial forces have pushed developers to add into their browsers--Netscape Navigator and Internet Explorer, in particular--nonstandard extensions meant to improve the language. Many times, these extensions are implementations of future standards still under debate. Extensions can foretell future standards because so many people use them.
In this book, we explore in detail the syntax, semantics, and idioms of HTML 3.2, along with the many important extensions that are supported in the latest versions of the most popular browsers, so that any aspiring HTML author can create fabulous documents with a minimum of effort.
Like many popular technologies, HTML started out as an informal specification used by only a few people. As more and more authors began to use the language, it became obvious that more formal means were needed to define and manage--to standardize--HTML's features, making it easier for everyone to create and share documents.
The World Wide Web Consortium
The World Wide Web Consortium (W3C) was formed with the charter to define the standard versions of HTML. Members are responsible for drafting, circulating for review, and modifying the standard based on cross-Internet feedback to best meet the needs of the many.
Beyond HTML, the W3C has the broader responsibility of standardizing any technology related to the World Wide Web; they manage the HTTP standard, as well as related standards for document addressing on the Web. And they solicit draft standards for extensions to existing Web technologies, such as internationalization of the HTML standard.
If you want to track HTML development and related technologies, contact the W3C at http://www.w3.org/. Several Internet newsgroups are devoted to the Web, each a part of the comp.infosystems.www hierarchy. These include comp.infosystems.www.authoring.html and comp.infosystems.www.authoring.images.
The Internet Engineering Task Force
Even broader in reach than W3C, the Internet Engineering Task Force (IETF) is responsible for defining and managing every aspect of Internet technology. The World Wide Web is just one small part under the purview of the IETF.
The IETF defines all of the technology of the Internet via official documents known as Requests For Comment, or RFCs. Individually numbered for easy reference, each RFC addresses a specific Internet technology--everything from the syntax of domain names and the allocation of IP addresses to the format of electronic mail messages.
To learn more about the IETF and follow the progress of various RFCs as they are circulated for review and revision, visit the IETF home page, http://www.ietf.org/.
Talking the Internet Talk HTML: What It Isn't


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DOJ OIG Releases Report on Two FBI Fuel Procurement Contracts with Petroleum Traders Corporation
The Department of Justice (DOJ) Office of the Inspector General (OIG) announced today the release of a report on two contracts between the Federal Bureau of Investigation (FBI) and Petroleum Traders Corporation (PTC), a wholesale supplier of gasoline and fuel products headquartered in Fort Wayne, Indiana, to purchase bulk automotive fuel for fleet vehicle use. One of the contracts was for the FBI Miami Field Office (FBI Miami) and the other was for the FBI Northern Virginia Resident Agency (FBI NVRA). The DOJ OIG audited these contracts for fiscal year 2015, during which the total amount expended by the FBI was $460,084.
The OIG's report identified several deficiencies with the FBI's contract award and administration processes that prevented the FBI from ensuring that it received the best fuel prices, received the proper amount of fuel at the agreed upon prices, and used the fuel in the most efficient manner. Specifically:
The FBI did not award the FBI Miami contract in accordance with the Federal Acquisition Regulation (FAR) that identifies the mandatory source to use for bulk fuel contracts.
FBI Miami purchased premium fuel, but the FBI could not support the need for this more costly fuel. We found that the FBI spent approximately $57,000 more on the premium fuel than it would have spent on regular fuel.
FBI contracting officers did not comply with the FAR in that they did not adequately review invoices or ensure the timely payment of invoices, and they did not maintain complete contract files and ensure the accuracy of information entered into the Federal Procurement Data System.
FBI contracting officers did not adequately verify the amount of fuel received as required by FBI policy.
While the deficiencies we identified were limited to the PTC contracts that we audited, we believe some of the issues could also exist with respect to other contracts through which the FBI purchases fuel in bulk.
In addition, we identified concerns about the location and security of the FBI Miami fuel pump. The fuel pump, located in Pembroke Pines, is a 12-mile roundtrip from the field office, which we found takes about 30 minutes. Moreover, the fuel pump and above-ground tank were not adequately secured, and FBI Miami had placed a sign on the fuel pump identifying it as an FBI pump.
Today's report makes 10 recommendations to the FBI that address the deficiencies we identified. The FBI agreed with all of the recommendations, and it has already taken corrective actions that were sufficient for the OIG to close three recommendations.
Today's report can be found on the OIG's website at the following link: https://oig.justice.gov/reports/2016/a1625.pdf.
PDF Press Release
2016-09-07a_1.pdf
Audit of the Federal Bureau of Investigation's Fuel Procurement Contracts Awarded to the Petroleum Traders Corporation


Breathtaking Mixed Flower Bouquet with Savoury Cake Appetizing Strawberry Cake Gorgeous Mixed Flowers Basket with Nutrtious Assorted Sweets. Delish Sweets and Flavourful Dry Fruits Hamper.
Seasonal Mixed Flowers Bouquet with 1 Lb Black Forest Cake 12 Yellow Roses with Cadbury Celebration and Kaju Katli Exquisite Mixed Flower Bouquet with Enticing Dry Fruits. Simply Amazing Cadburys Celebration Pack.
Mouthwatering Ferrero Rocher Chocolates with free Roli Tilak and Chawal Majestic Arrangement of 15 Gorgeous Roses with Teddy Floral surprises Fiery Red Rose Bouquet with Tasty Assorted Sweets and Dry Fruits.
Dry Fruits Bright Yellow Roses with Delicious Assorted Sweets Assorted Sweets Fresh Fruits and Amazing Flowers.
Bouquet of 12 Dutch Red Roses with 1 Lb Cake, Mixed Cadburys Chocolates and a Teddy Bear Fresh Orchids Basket and Tasty Kaju Katli. Delightful Kaju Kaltli with Dry Fruits 12 Beautiful Red Carnations Bouquet with Juicy Rasgulla.
Chocolate Flavor Eggless Cake Ravishing Mixed Dry Fruits. Appetizing Eggless Cake and Spectacular Mixed Flowers Bouquet.


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The Radical New Fentanyl Trend That Could Save Lives and Screw Dealers
One $5 or $10 fatal dose could become dozens or even hundreds of nonfatal highs.
by Maia Szalavitz
Nov 20 2018, 7:59pm
Left Image: A perceived heroin-fentanyl mix from Lawrence, Massachusetts. Photo by Dan Ciccarone. Right Image: Perceived fentanyl from Lowell, Massachusetts. Photo by Eliza Wheeler. Images courtesy Jeff Ondocsin
Mark Kinzly, a needle exchange worker in Austin, Texas, recently came across an opioid user who was doing what many thought impossible. The man claimed to be regularly taking carfentanil—a drug 10,000 times stronger than morphine and 100 times more potent than fentanyl—which is only approved for use in sedating large animals, like elephants. Carfentanil is typically found at autopsy in overdose victims, and not noted as a drug of choice.
Speaking at a session on fentanyls at the Harm Reduction Conference in New Orleans last month, Kinzly recalled that despite daily use, the guy was alive and seemingly OK. "He has figured out a way to take a certain amount of micrograms of the carfentanil, dilute it into a 50 milliliter solution of saline and basically draws it up a couple of times during the course of a day and injects it," he said.
"Economically, for this individual, the amount of micrograms that he pays about $250 for will last him about three months," Kinzly added. In other words, it was lemonade from lemons: making what could have been one deadly dose into a cheap, abundant supply that lasted for weeks. Typically, opioid users may spend around $100 or more per day on their drugs.
Faced with the literally poisonous level of potency of the opioids currently available on the street, most consumers have been hard-pressed to adapt. Nearly 30,000 fentanyl or fentanyl analog overdose deaths—more than any other drug and rising—last year was clear evidence of this.
But as people with addiction confront the daily risks posed by the fentanyl-tainted drug supply—mostly without access to evidence-based treatment even if they want it—they are taking new steps to protect themselves. The sheer danger associated with the potency of fentanyls and other powerful opioids is changing how people use drugs like heroin, and some of the strategies they're working on could upend the economics of drug sales.
Dilution is one of several techniques in what might be best categorized as the testing stage. As Kinzly put it, "It's a pretty common practice, starting to happen." And if this and other harm-reduction approaches were replicated reliably, they could both save lives and alter the market in ways that make fentanyl and its analogs much less profitable for dealers.
The principle behind dilution is simple: putting a tiny bit of a strong drug into a large amount of water makes it much less potent. As Biology 101 students know, in solution, even without being mixed, chemicals tend to diffuse out from regions of high concentration to those that are lower. And so rather than a lethally large dose, a properly diluted solution would offer many, many effective but (at least somewhat) safer ones. This, in fact, is how FDA-approved fentanyls can be—and are widely—used safely in medicine.
If dilution could be done properly on the street—and this is a big if, given that most people don't know how much of which kind of fentanyl is in their drugs and their potencies range widely, which makes it hard to determine how much water to add—it could have serious implications.
For starters, it might mean that one $5 or $10 fatal dose became dozens or even hundreds of nonfatal highs, depending on which type of fentanyl was in play. If users were to dilute drugs weaker than fentanyl, the result would obviously be a weaker high. But if they diluted synthetic, overdose-level opioids, as many as tens of thousands of effective doses could be present.
In this scenario, some people who now buy several times a day would, perhaps, buy weekly or less. Such market pressure might push dealers back to selling somewhat less potent (albeit still deadly) substances, like heroin. It could also compel them to cut fentanyls more effectively higher up the chain. (Or, it could lead to other unpredictable effects—like dealers doubling down on mainstays like coke.)
"I think dilution is a brilliant idea," said Maya Doe-Simkins, a public health consultant and director of communications for the Chicago Recovery Alliance, which provides harm-reduction services. "I mean, it makes perfect sense," she added, cautioning that supporting dilution as harm reduction would probably require supplies not currently stocked by needle exchanges. Saline solution, for example, would be needed instead of commonly used sterile water, in order to prevent bacteria from growing in solutions that might be stored for some time rather than injected immediately.
There's also the question of how users might react to having more drugs on hand than they could immediately consume. Some might just overdose more slowly by way of many shots rather than one more potent one. Still, the potential for harm reduction is real.
"I think [dilution] is an important consideration moving forward," Jeff Ondocsin, an ethnographer at the University of California San Francisco (UCSF) who's studying changes in the heroin market, told me. "I believe that fentanyls could be used safely if the dosage was correct and it wasn't a poisoning."
During the panel discussion, Ondocsin, and his colleagues Dan Ciccarone, professor of family and community medicine at UCSF and Sarah Mars, project director for their research, presented initial findings on geographic "hotspots" marked by swift changes in heroin markets. This "Heroin in Transition" project includes San Francisco, Chicago, Baltimore and Lawrence and Lowell in Massachusetts, and in-depth interviews had so far been conducted with 111 people who were taking heroin—or what was being sold as such—in those places, they said.
A number of strategies have emerged to contain street fentanyl's capacity to kill. The first and most effective was for people to never use alone—while keeping the antidote, naloxone, on hand in case of an overdose. Perhaps most obviously, it is better to avoid overdose than to have to reverse it.
But Ondocsin described several other techniques in use among research participants, whom he kept anonymous for ethical reasons but quoted during his talk. A man he called Riley from San Francisco, for example, discussed smoking a bit of his black tar heroin to see how strong it was before injecting. "I'll smoke it just to see how I feel from taking a couple of hits," Riley told researchers, adding that if he got "spooked" by how strong it seemed, he would inject much less than usual.
Other tactics that came up in the research included trying a very small "tester" injection first or snorting a small amount of the powder and getting a sense of how it tasted when it hit the back of the throat. One Chicago man told the researchers, "When you toot it's supposed to go down your nose and go down smooth with no burn and none of that, and once you get that drain, it's the taste. It tastes like dope." Rather than using a small initial shot, other people instead injected their dose extremely slowly, the research suggested, at least theoretically giving them time to pull out if the dose was too high.
The incredible variability of the heroin and fentanyls market loomed large. "I know a lot has been said about how potent fentanyl is," Ciccarone said at the panel. "But a bigger concern from a pharmacological point of view, if you will, is the changes in it… We gather these stories about how the substance itself changes on a daily basis."
This irregularity—in and of itself—may also be increasing overdose death risk via an effect it has on tolerance. After all, tolerance to a dose is produced by repeated exposure, which over time means that more of the same drug is needed to get the same effect.
But what causes tolerance to kick in is a process of learning: the response is elicited by cues associated with the drug, such as the place where you use it, the smell of the substance, its taste, and the sequence of the ritual connected with use. In a highly variable market where the drug's composition is constantly shifting, these cues may not be present. Blue heroin may not cause tolerance to occur as reliably as in a person who has only previously used white, for example.
The risk isn't just theoretical: One study found that if rats were given an opioid dose they were tolerant to in an unfamiliar cage, 50 percent would die even though they were taking exactly the same amount they'd survived in the past. Research on humans with alcohol—dubbed the "Four-Loko Effect"—has suggested people will get more drunk— in other words, have lower tolerance—if their beverages are extremely oddly colored and flavored in contrast with typical drinks.
This speaks to another harm-reduction tactic for the age of fentanyls: People are best off using with the same friends in the same place in the same way at the same time whenever possible, in order to maximize tolerance, by giving their bodies as many familiar cues as they can. (This is one way safe-injection facilities could help; another is providing test strips and other supplies that could bolster safer injection outside designated spaces.)
Ciccarone noted a telling phenomenon in fentanyl world: even now, these drugs often have no real street name. While the apt "null" and "nil" are heard in some regions, several years after heroin markets in the Eastern US were flooded with the stuff, fentanyls are mostly nameless or sold as heroin, he said. This may speak to both the rapidity and the variability through which the substances have changed the opioid crisis.
For his part, Ciccarone saw this as evidence of their unpopularity and the fact that they were introduced not because of new demand, but because they were cheaper to produce. "A drug that's popular, that people want, slang gets developed around it," he said. "There's not a lot of slang for fentanyl. Even the dealers were surprised." Though reports have begun to surface of people who actively seek it, many consumers do the opposite and avoid it: between 50 and 75 percent, according to Ondocsin's sample.
While it would obviously be better if fentanyls were not in the street opioid supply at all, if dilution made them safer and cheaper, it really might help ease the opioid crisis. Perhaps the dealers benefiting from opioid addiction at the street level would have to change up their strategy. We don't know exactly what that might look like, but almost anything would be better than what's going on now.
Follow Maia Szalavitz on Twitter.
VICE US


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ND Hockey Panoramic Win Over U-M
SKU 6653-UN
Notre Dame - Compton Family Ice Arena - White Out Night
Feb 8, 2013: Fighting Irish defeat Wolverines 7-4
This panorama, taken by Christopher Gjevre, captures the Notre Dame Fightin' Irish defeating their oldest hockey rival, the Michigan Wolverines, on White Out Night at Compton Family Ice Arena. The two teams first met during the 1921-22 season and have played each other over 130 times. Since ice hockey was first established at Notre Dame in 1912, the program has greatly evolved. Today, in its fifth decade at the Division I level and playing in the NCAA as a menber of the Central Collegiate Hockey Association (CCHA), the Irish have earned multiple NCAA Tournament and Frozen Four appearances. Starting in the 2013-14 season, Notre Dame will join Hockey East.
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TCEQ refers Acres Homes concrete batch plant dispute to state hearing
Erin Douglas Oct. 9, 2019 Updated: Oct. 9, 2019 6:25 p.m.
TCEQ refers Acres Homes concrete batch plant dispute to...
1of4Sen. John Whitmire (D-Houston), speaks during the Oct. 9 TCEQ Commissioners' Agenda Meeting in Austin, Texas.Photo: Marjorie Kamys / Marjorie Kamys Cotera
2of4Soto Ready Mix's site is shown from the yard of Donna and David Williams. Residents in the Acres Homes neighborhood have been fighting the concrete company's proposal to build a batch plant at the site for nearly two years. On Wednesday, the company withdrew its application.Photo: Steve Gonzales, Houston Chronicle / Staff photographer
3of4David Williams points out a damaged fence from concrete trucks hitting it. Soto Ready Mix purchased the land next door to the Williams a few years ago, and now the company wants to build a batch plant in the neighborhood.Photo: Steve Gonzales, Houston Chronicle / Staff photographer
4of4Area resident Ruby Glass asks questions during a public meeting with city and state agency representatives at the Acres Homes Multi Service Center about a proposed concrete batch plant in the Acres Homes residential area Monday, Jul. 22, 2019 in Houston, TX. Hundreds of residents have organized to contest the permit application.Photo: Michael Wyke / Contributor
The Texas Commission on Environmental Quality on Wednesday granted a hearing to residents in Houston's Acres Homes community fighting the placement of a concrete mixing plant in their neighborhood.
For nearly two years, hundreds of residents in the historically black neighborhood in northwest Houston have fought against an environmental permit for a small business, Soto Ready Mix, to build the plant in a residential area on De Soto Street.
Making concrete is a notoriously dusty process that spews small particles into the air, which, according to the Environmental Protection Agency, can cause asthma attacks, cardiac arrest and premature death, depending on how much is inhaled. The plant would be located just across the street from a park where children play and next door to a family home.
The decision by the TCEQ commissioners Wednesday will at least slow permit approval. The commissioners sent the issue to the State Office of Administrative Hearings, where a judge will hear arguments by affected residents and then make a recommendation of action to the TCEQ commissioners for the final decision.
Policymakers and residents made the trip to Austin to comment on the permit, which is seen by many as a test for the agency. The TCEQ has long been criticized by environmental activists for complacency in granting permits, which are rarely denied. Over the last five years, the TCEQ has received more than 100 requests for concrete batch plant air emissions permits in Houston, and only two were denied, according to the agency's records.
More on The Dispute on De Soto: One Houston neighborhood is putting Texas' air quality rules to the test
"We need to show people that we are responsive, and quite frankly, this agency is controversial," said state Sen. John Whitmire, D-Houston. "You have an opportunity to restore faith in this agency."
Many communities often are unaware of an environmental permit request nearby, or unable to organize enough opposition to fight it. But Acres Homes residents have done just the opposite, rallying politicians, forcing regulators to host several public meetings and engaging fully in the permit request process.
But that process is notoriously difficult to get through. Even though the TCEQ commissioners granted six people who live within 440 yards of the proposed plant (the technical requirement to be considered an "affected person") a hearing before an administrative judge, there's no guarantee the judge will rule in their favor. And, even if the judge sides with them and recommends the permit be rejected — the TCEQ's three commissioners, who are appointed by the governor, are under no obligation to heed the judge's advice in the final decision.
The hearing presents its own challenges. Before state law changed in 2015, it was the company's responsibility to defend its application at the hearing before a State Office of Administrative Hearings judge. Now, the burden is on the opposition to find errors in the application, meaning that residents must spend time and money on legal fees and expert witnesses to challenge the application.
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The plant permit request in Acres Homes exists in a sort of blind spot in state and city policies. The TCEQ has claimed it has no say over where plants are sited, which in Houston can be almost anywhere due to the city's lack of zoning laws.
"Don't fault the community for a government decision not to have zoning," U.S. Rep. Sheila Jackson Lee, D-Houston, told TCEQ commissioners Wednesday. "My constituents don't have fancy lawyers. I am disappointed in the fact that we have to be here at all."
Air quality is chief among the concerns of residents in the area. The area has double the rate of cardiac arrest and six times the rate of ambulance-treated asthma attacks than the rest of Houston, according to a study of 911 call data by the city of Houston. The neighborhood also has a high risk of cancer, according to Environmental Protection Agency data analyzed by the city. Residents are concerned that an additional emissions source will compound issues for a community that is already sensitive to poor air quality.
"It's the wrong application at the wrong place," Whitmire said. "I've represented this community for 47 years. I thought I'd seen everything until I saw this application. It is unconscionable."
erin.douglas@chron.com
Twitter.com/erinmdouglas23
Erin Douglas
Follow Erin on:
erinmdouglas23
Erin covers the local economy for the Houston Chronicle, focusing on energy and the environment. Previously, she interned for Bloomberg and The Denver Post. Erin is from Colorado and studied journalism and economics at Colorado State University. Reach her at erin.douglas@chron.com.
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Fortuna, California facts for kids
For the former town with this name in Fresno County, see Fargo, California.
City of Fortuna
Main Street Fortuna in the 1940s
Nickname(s):
The Friendly City
Location in Humboldt County and the state of California
4.845 sq mi (12.549 km2)
• Land
• Water
0 sq mi (0 km2) 0%
66 ft (20 m)
2,461.5/sq mi (950.35/km2)
UTC-8 (Pacific (PST))
UTC-7 (PDT)
FIPS code
GNIS feature IDs
Fortuna (formerly, Slide, Springville) (Wiyot: Vutsuwitk Da'l, "ashes stay") is a city the northeast shore of the Eel River (approximately 9 miles (14 km) from where it enters the Pacific Ocean), and is on U.S. Route 101 in west-central Humboldt County, California, United States. The population was 11,926 at the 2010 census, up from 10,497 at the 2000 census.
The settlement was originally called "Slide," for Slide Hill, in 1874, named for the slide that was a fixture on the northeast side of the Eel River and the southwest portion of Christian Ridge just to the northwest, near the edge of town. In 1875, the name was changed to Springville during the construction of the Springville Mill, a lumber mill for the nearby redwood forests, named so because of the numerous springs in the area. The mill's owners were Henry Rohner (namesake of neighboring Rohnerville), Alexander Masson, M. N. Weber and G. F. Gushaw. Springville was originally a company town belonging to the mill, and the few people that resided there all worked at the mill. By the late 1870s Springville had grown enough to warrant a post office, but a town called Springville, California (now part of Camarillo, in Ventura County) already existed in the state. The post office was named Slide on May 24, 1876. In 1884 the residents petitioned the state legislature for the name Fortuna, Spanish for "fortune" and Latin for "chance," and by July 3, 1888 the name was changed to Fortuna. The name was chosen when settlers saw the proximity of the forests, the river and its valley, and the Pacific Ocean, as ideal for enjoying a good quality of life, and felt "fortunate" to live there. It is believed that a local minister and real estate agent, desiring to sell lots to newcomers, devised the name as a marketing tool.
Electricity came to Fortuna in 1883 when W. J. Swortzel and George W. Williams (of Swortzel & Williams), owners of the Springville Mill Company, built a $4,000 power plant. Some of the local sawmills were already powered by electricity, and by providing power to the mills, Swortzel and Williams saw the opportunity to also provide inexpensive electric lighting to the townspeople.
The town was incorporated on February 20, 1906, and, because of the Eel River, became known for its agricultural prowess in vegetable crops, berries and fruits, and for the fresh fish from the river. Although agricultural industry was expanding, the lumber industry is what started the town, and would continue as the main source of local income for some time to come.
Rohnerville (formerly Eel River Township), a town founded to service the many gold miners inhabiting the mountains to the north and east, was competing with Fortuna to be the leading township in the area. The miners would come by ship to Eureka, and then head up the Eel River to the junction with the Van Duzen River, from whence the miners headed east up the Van Duzen River Valley into Trinity County. Rohnerville was at this junction, and looked to prosper from selling supplies to the miners. But when it was decided that the railroad would be routed through neighboring Fortuna, it set both towns' fate.
The Eel River and Eureka Railroad was built in 1884 to provide Humboldt Bay shipping access to the lumber mills and farms of the lower Eel River. Atchison, Topeka and Santa Fe Railway reorganized Fortuna's railroad as the San Francisco and Northwestern Railway in 1903, and then completed the Northwestern Pacific Railroad to San Francisco in 1914. Fortuna became the rail hub for smaller communities like Alton, Fernbridge, Ferndale, Hydesville, Newburg, Port Kenyon, Rohnerville, and Waddington. Fortuna was the location of one of two secondary mills of the storied Pacific Lumber Company, headquartered ten miles south in Scotia.
Since Fortuna's earliest days in the 1800s, its nickname has been "The Friendly City."
According to the United States Census Bureau, the city has a total area of 4.8 square miles (12 km2), all of it land.
Fortuna is located 7 miles (11 km) from the Pacific coast on the bank of the Eel River. The community is affected by coastal weather patterns with the Pacific Ocean to the west. Fortuna is served by U.S. Route 101 providing direct access to San Francisco 253 miles (407 km) to the south, and to Eureka (County Seat) 14 miles (23 km) to the north. The western terminus of California State Route 36 intersects U.S. Route 101 1 mile (1.6 km) just south of the city limits. Fortuna is surrounded by national, state and county redwood parks, and is the gateway to the redwood forests of Northern California. Sequoia sempervirens grow to about 300 feet (91 m) and live to be 2,500 years old. The 33-mile (53 km) Avenue of the Giants offers one of the most spectacular views of the redwoods as it carries visitors through grove after grove. Stops include Founders Grove, the Visitor Center near Weott and several locations that provide trail access.
Historical population
1910 383 —
1920 986 157.4%
1930 1,239 25.7%
2000 10,497 19.4%
Est. 2015 12,000 0.6%
U.S. Decennial Census
The 2010 United States Census reported that Fortuna had a population of 11,926. The population density was 2,461.4 people per square mile (950.3/km²). The racial makeup of Fortuna was 9,686 (81.2%) White, 73 (0.6%) African American, 444 (3.7%) Native American, 106 (0.9%) Asian, 9 (0.1%) Pacific Islander, 1,065 (8.9%) from other races, and 543 (4.6%) from two or more races. Hispanic or Latino of any race were 2,032 persons (17.0%).
Twenty thousand visitors fill the town during Fortuna's Redwood AutoXpo
The city has a large number of events and festivals including the Daffodil Festival, Art & Wine in the Park, the Annual Fortuna Rodeo, the Redwood AutoXpo, the Logging Competition, Civil War Days, and Apple Harvest, the Hops in Humboldt festival, the Fortuna Concert Series and holiday events including concerts and parades with performances by Scotia Band Brass Choir and Saxophone Quartet. Additionally, the Eel River was the locale for the Paddle to the Headwaters canoe race.
River Lodge attracts meetings and events.
Fortuna, California Facts for Kids. Kiddle Encyclopedia.


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In Topics in Cryptology - CT-RSA 2011, The Cryptographers Track at the RSA Conference 2011 Volume 6558 of LNCS , page 161-179.
In Proceedings of the 18th ACM Conference on Computer and Communications Security (CCS 2011) , page 41-50.
in ASIA CCS'11: 6th ACM Symposium on Information, Computer and Communications Security, , page 176-185.
Securing Electronic Business Processes Volume 2010 of ISSE , page 26-38.


We had a big turnaround in the financials today which brought the whole market up. The market decided, somehow, that a 10% drop in MER, Merrill Lynch was enough of a drop. It is not totally surprising because the financial stocks have been beaten down for so many months, over a year for MER from $95 to $20 in stock price.
It is very common that an "event" causes a stock to have a reversal, call it a catalyst. It was enough to turn on the buy programs for all the financials and it carried over to virtually all sectors except the oil stocks.
I covered the BAC short this morning just under $28 and sold the SKF at $143.80 within 25 minutes of the regular opening. The clues were that financials looked like they were bottoming and my eyes were especially glued to MER. I thought that if MER had a big drop it would be likely at the opening. It had a delayed opening and gapped down to about $22 and immediately started up with subsequent higher highs.
Virtually all the financials were heading up together in that first 30 minutes because they are linked together on buy programs. SKF couldn't get much above $144 so I pulled the trigger on both. I did not short SKF and was surprised it dropped so much but it is a leveraged fund.
If financials follow through tomorrow (Wednesday, July 30th) in a substantial way, like WFC over $32.50 and BAC over $36, then I would look at shorting them again for a few days but this is a very aggressive idea usually for experienced traders. If this set-up does occur, then a very small portion of funds should be used for this trade.
I am not convinced that everything is alright with the world of financials so I expect the volatility will still hang around for another week or so in this sector.
Oil dropped 2% today and the technical indicators are signaling that we should be having a substantial rebound and may result in a rebound back up 10-12%. I think we have very high odds that we will see this rebound start within the next few days. It won't take much to trigger it and we don' t necessarily need political unrest, or some trigger point in news to cause a rebound.
This is sort of a Mitch King rule that I have for myself. When you see a sector that has had a big run-up like oil has had this year, the first big drop usually has strong rebound caused by short covering and speculative buying from those who "lost out" on the first big run. In other words, people just don't leave a sector like this all at once and the stock goes down without a partial rebound. An individual stock can do that if there is something like accounting irregularities, fraud, or government action against a specific company.
Besides, the indicators on the charts just look really good. A reader emailed me a good looking chart for an oil long candidate, XTO.
I modified last night's list of independent oil and gas stocks. There are a lot more than this available but look at these as very good ideas for long purchases that may last several weeks of moving up.
CLHB, Clean Harbor is a type of chart that is on a sustainable run upward. It is good to buy strong stocks when they have been going up in a down market. When the market turns around with a general uptrend, these strong stocks like this tend to continue an upward trend. This may have a few down days before potentially resuming upward again so let's say $74 is an entry point for example. A stop loss of maybe $1.50 would be appropriate.
ACOR, Acorda Therapeutics is a biotech company and this sector has been getting a lot of money this past couple of months.
NOTE: I have received a few requests for a workshop so if we can get a few people together at my house in West Linn Oregon next Saturday, August 9th for the full day, I have a very comfortable large living room to teach with a LCD projector, sceen and one of my desktop computers. If you have a laptop and can download the software from the brokerage firm you use, I can help you set that up with charts. There are chart set-up instructions with all 5 major online brokerage firms in the members area or I can email them to you directly as well. Cost is $399, bring a sack lunch because we live out in the country so driving somewhere to eat is inconvenient. Email me at mitch@tradestocksamerica.com if you can make it.


Since World War II, abortion policies have remained remarkably varied across European nations, with struggles over abortion rights at the forefront of national politics. This volume analyses European abortion governance and explores how social movements, political groups, and individuals use protests and resistance to influence abortion policy. Drawing on case studies from Italy, Spain, Norway, Poland, Romania, Russia, Sweden, Switzerland, the United Kingdom and the European Union, it analyses the strategies and discourses of groups seeking to liberalise or restrict reproductive rights. It also illuminates the ways that reproductive rights politics intersect with demographic anxieties, as well as the rising nationalisms and xenophobia related to austerity policies, mass migration and the recent terrorist attacks in Europe.
Silvia De Zordo is a Senior Researcher at the University of Barcelona (UB), Department of Anthropology. Her research interests encompass contraception, abortion and conscientious objection in Latin America and Europe. She has recently been awarded an ERC Starting Grant to study the impact on women of barriers to legal abortion in Europe. Her recent publications include Reproduction and Biopolitics: Ethnographies of Governance, "Irrationality" and Resistance (ed. with Milena Marchesi), published by Routledge in 2014.
Joanna Mishtal is an Associate Professor of Anthropology at the University of Central Florida. Her research examines reproductive rights, health, and policies in Poland, and in the context of EU governance. Her ethnography The Politics of Morality: The Church, the State and Reproductive Rights in Postsocialist Poland (2015) received the Adele E. Clarke Book Award in 2017.
Lorena Anton is a Marie Curie Fellow in social anthropology at the University of Bucharest (2013-2017), where she develops a project on abortion governance in post-communist Romania. Recent publications include 'On n'en parlera jamais de tout ça! Ethnographier la mémoire de l'avortement en Roumanie de Ceaușescu', in Ethnologie Française (2014) and the 'Cultural Memory' entry in Protest Cultures: A Companion (eds. Fahlenbrach et al., Berghahn Books).