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

The subdwarf B (sdB) stars are core helium-burning objects with envelopes that
are too thin to sustain nuclear burning \citep[e.g.\ ][]{Heber86}. They can be
identified with models of Extreme Horizontal Branch (EHB) stars; in other
words, they have masses $\sim$0.5\,$M_\odot$ and will evolve directly to the
white dwarf cooling curve, bypassing the Asymptotic Giant Branch. While their
future evolution seems secure, the formation of these stars is uncertain. In
recent years radial velocity surveys have shown that a large fraction of sdBs
are in short-period binary systems \citep{MHMN01}, it appears certain that
binary interaction plays a significant role, however many objects are
apparently single. A binary population synthesis study by \citet{HanII} has
found that three channels can give rise to the observed characteristics of
sdBs: one or two phases of common envelope evolution; stable Roche lobe
overflow; and the merger of two helium-core white dwarfs. The latter scenario
could explain the population of single stars.

The possibility of pulsations in sdB stars was theoretically predicted by
\citet{CFB96} at around the same time they were observed by
\citet{ECpaperI}. The more than 30 known pulsators (officially known as
V361\,Hya stars) have $T_{\mathrm{eff}}=29\,000-35\,000$\,K and
$\log g=5.2-6.0$, periods of 1-10 minutes and amplitudes less than 60\,mmag
\cite[see ][for a review]{Kilkenny2002}. The driving mechanism of the
oscillations is believed to be related to the ionisation of iron and other
heavy elements at the base of the photosphere \citep{CFB97a}. As is the case
for other types of pulsators \citep[e.g.\ the PG~1159 stars,][]{QFB04} there is
an overlap in the ($T_{\mathrm{eff}}, \log g$) plane between pulsators and
non-pulsators \citep{ECpaperXII}. Diffusion calculations by \citet{CFB97a}
suggest that the surface iron abundance of pulsators should be higher than
that of non-pulsators, however studies by \citet{EHN06}, \citet{HE04} and
\citet[][ hereafter HRW]{HRW00} find that iron has approximately solar
abundance in most sdBs.

For this reason we set out to determine if any correlation exists between
surface abundances of iron-group elements for pulsators and
non-pulsators. Since elements such as nickel, manganese and chromium are not
normally accessible through ground-based optical spectra, it was necessary to
acquire high-resolution UV echelle spectra with the \emph{Space Telescope
  Imaging Spectrograph} onboard the \emph{Hubble Space Telescope}
(\emph{HST/STIS}). If it is not possible to separate
groups based on abundances, perhaps differing mass-loss rates contribute
significantly, as suggested by \citet{FC97}. Regardless of this, our abundance
measurements will be extremely useful for testing diffusion theory. Previous
studies of sdBs using UV spectra from the \emph{International Ultraviolet
  Explorer} (\emph{IUE}) suffered from mediocre S/N as well as
from poor, or a lack of, atomic data; this was especially the case for the
iron group \citep[e.g.\ ][]{BHS82,BSK82}.

\begin{table*}
\caption{Observations of six sdB stars using \emph{HST/STIS}. Note that
  CPD~$-64^\circ 481$\ was observed only in the FUV and using the E140H grating.}
\label{tab:obs}
\begin{center}
\begin{tabular*}{1.00\textwidth}{l|cccccccccc}
Target & $\alpha$ & $\delta$ & $V$ & $T_{\mathrm{eff}}$ & $\log g$ & log(He/H)
& Ref. & Pulsator? & $T_{exp}^{NUV}$ & $T_{exp}^{FUV}$ \\
       & (2000)   & (2000)   & (mag) & (K) & & & & & (s) & (s) \\
\hline
PG~1219$+$534 & 12 21 29.1 & +53 04 37 & 13.2 & 33\,500 & 5.87 & $-$1.6
& 4 & yes & 3100/3100 & 2160/3100 \\
Feige~48     & 11 47 14.5 & +61 15 32 & 13.5 & 29\,500 & 5.54 & $-$2.9
& 2 & yes & 3500/3511 & 3600/3600 \\
CPD~$-64^\circ 481$ & 05 47 59.3 & -64 23 03 & 11.3 & 27\,500 & 5.60 & $-$2.5 & 3 & no & --- &
1440 \\
Feige~66     & 12 37 23.5 & +25 03 60 & 10.6 & 34\,500 & 5.83 & $-$1.6 & 4
& no & 824 & 875 \\
CD~$-24^\circ 731$       & 01 43 48.6 & $-$24 05 10 & 11.0 & 35\,400  & 5.90 & $-$2.9 & 4
& no & 800 & 878 \\
\hline
\end{tabular*}
\end{center}
References: (1) \citet{HRW99}; (2) \citet{HRW00}; (3) \citet{OJF05}; (4) This
work.
\end{table*}

The  two pulsators we have chosen to observe are
Feige~48 \citep{ECpaperXI},  and
PG~1219$+$534\ \citep{ECpaperXII}.
Quantitative analysis of the first two objects using optical
spectra was carried out by HRW and the latter by \citet{HRW99}. As comparison
objects we have chosen Feige~66 and CD~$-24^\circ 731$\ (alias SB~707); a high-resolution \emph{IUE}
spectrum of the former was analysed by \citet{BHS82}. A very high-resolution
spectrum of the sdB CPD~$-64^\circ 481$\ was found in the \emph{HST} archive;
since its temperature is close to that of Feige~48, and it is not pulsating
(Koen, private communication), we decided to use it as a comparison
star to Feige~48. Note that these two stars, along with CD~$-24^\circ 731$, are in
close binaries. Feige~48 and CPD~$-64^\circ 481$\ have periods of 0.376\,d and
0.2772\,d respectively, while CD~$-24^\circ 731$\ has a period of 5.85\,d
\citep{OHB04,EHA05}. The companions of Feige~48 and CD~$-24^\circ 731$\ are both
most likely white dwarfs, while the nature of the companion of
CPD~$-64^\circ 481$\ is uncertain.

In this paper we present a detailed abundance analysis of each of these
objects
based on UV echelle
spectra obtained using \emph{HST/STIS}. We discuss the possible
correlation between iron-group abundances and pulsation, the
abundances of heavy elements in the context of radiative acceleration
and the trends discussed by \citet{SJOT04}, and
a solution to the temperature discrepancy seen between Balmer line fitting and
helium ionisation equilibrium.

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

Observations were made using the \emph{Space Telescope Imaging Spectrograph}
(\emph{STIS}) onboard the \emph{Hubble Space Telescope} (\emph{HST}). We
observed five stars, three pulsators and two non-pulsators for comparison. One
of the non-pulsators, Feige 66 is a spectroscopic twin of one of the pulsator
PG~1219$+$534. Details of the observations are shown in Table \ref{tab:obs}.
The stars were observed in the near- and far-UV (NUV and FUV) using the medium
resolution echelle E140M and E230M grisms. The NUV spectra each have a central
wavelength of 1978\,\AA, covering the wavelength range 1700-2370\,\AA, while
the FUV spectra are centered on 1425\,\AA, covering the 1160-1730\,\AA\
range. For all spectra a slit width of 0.2''$\times$0.06'' was
used. Each pulsator was observed in time-tag mode, where the
arrival times of each photon is recorded; the two non-pulsators were observed
in histogram mode. The spectra of Feige 48 have yielded one piece of
serendipity -- the discovery of velocity variations indicating a binary
companion to the star \citep{OHB04}.
Additionally, we found very high-resolution spectra
of Feige~66 and CPD~$-64^\circ 481$, taken using the E140H grism with a
0.2''$\times$0.2'' slit covering the range 1163-1363\,\AA. All of the
spectra are sharp-lined as expected from the low projected rotation
velocities seen in sdBs \citep[][and HRW]{OHB04}.

\section{Synthetic spectra}
\label{sec:synth}
In hot subdwarfs, most of the spectral lines due to iron-group
elements (V, Cr, Mn, Fe, Co, Ni) are found blueward of $\sim$2300\,\AA,
and in many cases continuum definition is difficult at the resolution
of our spectra. The methods we used to get around these problems are
discussed in more detail in Section \ref{sub:contdef}.

As input for our spectrum synthesis, we used a metal line-blanketed LTE model
atmosphere with solar metalicity and Kurucz' ATLAS6 Opacity Distribution
Functions. The spectra were synthesised using Michael Lemke's version of the
LINFOR program (originally developed by Holweger, Steffen, and
Steenbock at Kiel University). Oscillator strengths were taken from
the Kurucz line list, as were damping constants for all metal
lines. Only lines that have been observed experimentally were used, since we
required the most accurate wavelengths possible. In the case of species
heavier than Zn, values were taken from the resonance line lists
of \citet{Morton2000,Morton2003}. For the partition functions of
Ga\,\textsc{iii}, Ge\,\textsc{iv}, Sn\,\textsc{iv} and Pb\,\textsc{iv}
we used these ions' ground state statistical weight, since no
published data is available. This is a good approximation at
temperatures of 30\,000-35\,000\,K. The Cu\,\textsc{iii} atomic data were
taken from the tables of \citet{HH95}. Oscillator strengths for
Ti\,\textsc{iii} lines were taken from \citet{RU97}. Lines
with $\lambda>2000$\,\AA\ were converted from air to vacuum wavelengths
using the formula of \citet{Edlen1966}.

\subsection{Atmospheric parameters}
\label{sec:atmospar}

The determination of atmospheric parameters for the two pulsators to
be discussed here was presented by HRW (the values are shown in Table
\ref{tab:obs}).
We selected Feige~66 and CD~$-24^\circ 731$\ as potential comparison stars for the
pulsator PG~1219$+$534\ because they are not known to pulsate and
published temperatures and gravities are similar to those of the latter.
While PG~1219$+$534\ has $T_{\mathrm{eff}}=33\,500$\,K, $\log g=5.85$
from Balmer line analysis by HRW, Feige~66 has
$T_{\mathrm{eff}}=33\,400$\,K, $\log g=6.2$ \citep{SBK94}
and CD~$-24^\circ 731$\ has $T_{\mathrm{eff}}=34\,000$\,K, $\log g=6.0$ \citep{HHJ84}.

For this work we have reanalysed the Keck-HIRES spectrum of PG~1219$+$534\ from
HRW. A high resolution (0.1\AA) optical spectrum of CD~$-24^\circ 731$\ was kindly
provided by M.\ Altmann and H.\ Edelmann. It was taken with the FEROS
spectrograph at the ESO 2.2m telescope. A low resolution (5\AA)
spectrum of Feige~66 taken with the CAFOS spectrograph was provided by
M.\ Altmann. The spectral analysis of both spectra
is described below. The parameters for CPD~$-64^\circ 481$\ have already been
determined by \citet{OJF05}.

\subsection{The hot sdB temperature discrepancy}
\label{sub:tempfix}

As has been noted by HRW, there is a discrepancy between temperatures
derived from Balmer line fitting and helium ionisation equilibrium. For
PG~1219$+$534, the difference in $T_{\mathrm{eff}}$ is 2000\,K.

After the initial discovery of strongly supersolar abundances of heavy
metals  in three of the programme stars (Feige 66, CD~$-24^\circ 731$\ \&
PG~1219$+$534), we  investigated how this affects the determination of
the atmospheric  parameters. HRW used metal-line blanketed models with
solar metal content. Using the same model
atmospheres described above but with metals scaled by a factor of 10
([M/H]=1.0), we have recalculated both our abundances and stellar
parameters ($T_{\mathrm{eff}}, \log g$). There are currently no
opacity distribution functions with higher metalicities. Also,
despite the fact that iron itself is show roughly solar abundances for
all our targets, in many cases the nickel abundances is 1-2 dex above
solar. It is possible that in these cases nickel may become the
dominant source of line opacity.

In Figure \ref{fig:pgp1fit} we show a fit with these models to the
optical spectrum of PG~1219$+$534. The Balmer lines and the
He\,\textsc{ii} can now be matched simultaneously. The parameters we
derive with our metal-enhanced models using all lines are closest
(within errors) to those found by
fitting the Balmer lines only with a solar-metalicity model. The
He\,\textsc{i} lines agree reasonably well, although the line cores of
the strongest lines match poorly. We expect ultimately the solution
will be found using opacity sampled models that can allow for enhanced
abundances relative to iron.

\begin{figure}
\vspace{9cm}
\begin{center}
    \special{psfile=3948fig1.eps hscale=48 vscale=48 hoffset=-25
    voffset=-90 angle=360}
\end{center}
\caption{Line profile fit for PG~1219$+$534\ using solar metalicity
  models (\emph{top panel}) and metal-rich models (10 times solar,
  \emph{bottom panels}). The Balmer lines and He\,\textsc{ii} at
  4686\,\AA\ match simultaneously when using the metal rich models
  (see text).}
\label{fig:pgp1fit}
\end{figure}

\begin{figure}
\vspace{9cm}
\begin{center}
    \special{psfile=3948fig2.eps hscale=48 vscale=48 hoffset=-25
    voffset=-90 angle=360}
\end{center}
\caption{Same as Figure \ref{fig:pgp1fit} but for CD~$-24^\circ 731$.}
\label{fig:p1fit}
\end{figure}

For CD~$-24^\circ 731$\ we found the same mismatch of the helium ionisation equilibrium
as for PG~1219$+$534\ when solar metalicity models were used (see Figure
\ref{fig:p1fit}).  Again this
problem is remedied by using metal-enriched models. In this case
a significantly higher effective temperature was derived from
the metal-enriched models than from the solar metalicity ones,
i.e. $T_{\mathrm{eff}}=35\,400$\,K compared with
$T_{\mathrm{eff}}=33\,800$\,K. CD~$-24^\circ 731$\ is a rather helium poor star
compared to Feige~66 and PG~1219$+$534, which might explain the different
metallicity dependence of the results. In addition, CD~$-24^\circ 731$\ resides in a
close binary system ($P$=5.85\,d), whereas Feige~66
is not known to be variable (E. Green, private communication). PG~1219$+$534\ is
also not known to be a radial velocity variable.

The low resolution spectrum of Feige~66 was analysed in the same way with
the metal-enriched models and we derived $T_{\mathrm{eff}}=34500$\,K,
$\log g=5.83$, log(He/H)=$-$1.6. In this case the parameters
agree with those found using non-LTE models; however, the He\,\textsc{ii}
4686\AA\ line does not agree with observations in the enhanced
metallicity case, but does in the non-LTE case. A high-resolution
spectrum is urgently required to resolve this issue.

The results of the new spectral analyses of PG~1219$+$534, CD~$-24^\circ 731$\ and Feige~66
revealed that their surface gravities are identical. The helium abundances
of PG~1219$+$534\ and Feige~66 are also identical, whereas helium abundance of
CD~$-24^\circ 731$\ is much lower than for the other two.
Their effective temperatures, however, are not identical as suggested by
the earlier spectral analyses. Feige~66 and CD~$-24^\circ 731$\ are hotter than
PG~1219$+$534\ by 1000K and 1900K, respectively.

The temperatures we derive here match those determined using metal-free,
non-LTE models by HRW. Recently, \citet{CFB05} used \textsc{Tlusty} and
\textsc{Synspec} NLTE models and confirm the NLTE results of HRW for
PG~1219$+$534\ to within 500\,K and 0.04 dex.
Since the heavy metal abundances of Feige~48 and
CPD~$-64^\circ 481$\ are much closer to solar than those of the former, a
reanalysis of these stars is not necessary. The abundances shown in
Table \ref{tab:4abu} are derived from models with these parameters.

\section{Line identification}
\label{sec:lineID}

As has already been noted, previous studies of high resolution UV
spectra of hot subdwarfs have suffered from poor, or a lack of, atomic
data. While the current situation is by no means perfect, we have
endeavoured to identify as many spectral lines as possible, and then
from these we have chosen suitable lines to measure
equivalent widths or carry out spectrum fitting. Our method is outlined
below, beginning with a brief discussion of the problems encountered
with continuum definition.

\subsection{Defining the continuum}
\label{sub:contdef}

\begin{figure}
\vspace{6cm}
\begin{center}
    \special{psfile=3948fig3.eps hscale=48 vscale=48 hoffset=10
    voffset=-10 angle=360}
  \end{center}
  \caption{Comparison of a 15\,\AA\ wide section of the near- and far-UV
  spectrum of PG~1219$+$534. In the NUV it is possible to measure the continuum
  level, while in the FUV it must be estimated. Note also the higher flux in
  the FUV.}
  \label{fig:compspec}
\end{figure}

In each of our spectra, the continuum is well-defined in the NUV,
especially redward of 2000\,\AA, allowing equivalent widths to be
measured. An example of the difference between crowded and
well-defined is shown in Figure \ref{fig:compspec}. There are also some regions
below 2000\,\AA\ where equivalent width measurements are possible. In
order to define the continuum in crowded regions, we measured
equivalent widths of all unblended lines and then generated synthetic
spectra using the abundances derived from this analysis; the continuum
of the crowded regions was set by matching the synthetic spectra to
the observations using a ``chi-by-eye'' fit. This was not always
straightforward however, since many lines still suffer from imprecise
atomic data, and some resonance line profiles are not well reproduced
in our assumed LTE atmosphere (see Section \ref{sub:nlte} for more discussion
and examples of this effect). Nevertheless there were almost always
enough useful lines for our method to be successful. Note that we are
not relying on precise knowledge of the star's $U$, $B$, or $V$
magnitude -- which is not always available; PG~1219$+$534\ is one case
-- to calibrate the model flux.

\subsection{Unblended lines}
\label{sub:unblend}

There are various line lists available for the analysis of stellar
spectra; most commonly used is the Kurucz list, although during our
analysis we found that often more accurate oscillator strengths and
wavelengths are available in other databases (e.g.\ \citet{HH95}). In
particular we found that several Co lines had poor term
identifications in the Kurucz list, Fe oscillator strengths were often
out of date, while oscillator strengths for Ti\,\textsc{iii} were
completely inconsistent with our observations.

To determine which lines in our spectra are not blended, we generated
synthetic spectra using only those lines in the Kurucz list that have
been observed experimentally and compared these directly with our
observations. If the continuum was clear on either side of the line
wings, and our line list showed only one possible match, we considered
it to be unblended. Lines that were visibly blended (e.g.\ with overlapping
wings) were ruled out for equivalent width measurement where the blend
could not be be identified.

\subsection{Individual elements}
\label{sub:indiel}

In many regions of our spectra, line blending is extremely severe,
which means that continuum definition is difficult (as discussed
above) and/or that many features are identified with more than one
ion. In this section we discuss the ions we have identified.

\subsubsection{C and N}

\begin{figure}
\vspace{6cm}
\begin{center}
    \special{psfile=3948fig4.eps hscale=50 vscale=50 hoffset=-10 voffset=-10
    angle=0}
\end{center}
\caption{Spectrum fit to the C\,\textsc{iii} multiplet at
  1174-1177\,\AA for Feige~48. The model is shown as the thick line. Other
  strong lines due to Cr\,\textsc{iv} and Fe\,\textsc{iv} are marked.}
\label{fig:f48c3}
\end{figure}

PG~1219$+$534\ and CD~$-24^\circ 731$\ do not show any carbon lines. In
CPD~$-64^\circ 481$\ the C\,\textsc{iii} lines at
1247 and 2297\,\AA\ are present, along with the 1176\,\AA\ multiplet,
while in Feige~48 and Feige~66 these C\,\textsc{iii} lines and the
C\,\textsc{iv} resonance lines around 1550\,\AA\ are seen. Figure
\ref{fig:f48c3} shows the 1176\,\AA\ multiplet of Feige~48 together
with a model spectrum fit; results from spectrum fitting are discussed
further in Section \ref{sec:abu}.

As found in almost all other sdBs, nitrogen lines are strong in our
spectra, although there are fewer lines than seen in optical
spectra. In our two cooler targets, N\,\textsc{iii} lines are visible
at 1183-1184\,\AA\, while the N\,\textsc{iv} line at
1718\,\AA\ is present in Feige~48. In
Feige~66, PG~1219$+$534\ and CD~$-24^\circ 731$, lines of N\,\textsc{iii} and
N\,\textsc{iv}, as well as the N\,\textsc{v} resonance lines can be
seen.

\subsubsection{Al and Si}

As has been noted by several authors \citep[e.g.][]{MontrealIII,MontrealV},
the abundance of silicon in sdB stars drops sharply at
$\sim$32\,000\,K. This is also the case for aluminum, although the
available upper limits on abundances are not as strict as for silicon.

Silicon in hot subdwarfs has been discussed in more detail recently by
\citet{SJOT04} and the objects studied here follow previously seen trends. The
detection of the Si\,\textsc{iv} resonance line in PG~1219$+$534\ is discussed
further in Section \ref{sub:comparison}. The Al\,\textsc{iii}
resonance lines are only detectable in Feige~48, although for
CPD~$-64^\circ 481$\ the relevant wavelength range is not covered by our spectra.

\begin{figure}
\vspace{6cm}
\begin{center}
    \special{psfile=3948fig5.eps hscale=48 vscale=48 hoffset=10
    voffset=-10 angle=360}
\end{center}
\caption{The S\,\textsc{iii} resonance lines for CPD~$-64^\circ 481$, showing an
  excellent match. The line at $\sim$1194.5\,\AA is one of the Si\,\textsc{ii}
  resonance lines, while the strong line at $\sim$1194.15\,\AA is unidentified.}
\label{fig:SIII}
\end{figure}

\begin{figure}
\vspace{6cm}
\begin{center}
    \special{psfile=3948fig6.eps hscale=48 vscale=48 hoffset=10
    voffset=-10 angle=360}
\end{center}
\caption{A region of spectrum showing blended iron-group lines for
  Feige~48, PG~1219$+$534\ and Feige~66. The line at $\sim$1858.2\,\AA\ is unidentified.}
\label{fig:fe1860}
\end{figure}

\subsubsection{S, Ar, Ca}

The higher resolution of our spectrum of CPD~$-64^\circ 481$\ allows us to clearly
distinguish the S\,\textsc{iii} resonance lines (shown in Figure
\ref{fig:SIII}). Because of severe crowding and lower resolution, this
is not possible in the case of Feige~48. The crowding is less severe
for PG~1219$+$534, Feige~66 and CD~$-24^\circ 731$\ -- although in the latter the
lines are weak -- so it is possible to make out the S\,\textsc{iii}
lines.

Ar\,\textsc{iii} lines are difficult to measure as they are all quite weak,
and often blended with lines due to iron-group elements. Despite this, we
could measure four lines in Feige~66 and one in PG~1219$+$534; the
other stars have only upper limits.

In the case of calcium, we were able to measure lines of
Ca\,\textsc{iii} for Feige~66, CD~$-24^\circ 731$\ and PG~1219$+$534. In
the cooler pair the Ca lines are either very weak or blended, making
measurements difficult.

\subsubsection{The iron group}

Lines of the iron group elements often lie at similar
  wavelengths, making it difficult to measure equivalent widths, and
  necessitating an analysis by spectrum synthesis. An example of this
  can be seen in the 4\,\AA-wide spectrum slices shown in Figure
  \ref{fig:fe1860}.

\textit{Scandium}: There are very few Sc\,\textsc{iii} lines available to
measure in our spectra, making abundances very difficult to measure.
It was only possible to measure the
resonance lines at 1603.064\,\AA\ and 1610.194\,\AA\ for Feige~66 and
CD~$-24^\circ 731$. For Feige~48 and PG~1219$+$534\ we could only place upper
limits, and our spectrum of CPD~$-64^\circ 481$\ does not cover these
lines.

\textit{Titanium}: The Ti\,\textsc{iii} resonance lines are present in
the spectrum of each star. Some subordinate lines are also
measurable. We note here that the oscillator strengths found in the
Kurucz line list are inconsistent with our observations. Therefore we
have used the values given by \citet{RU97}, which match significantly better.

\textit{Vanadium}: Lines of V\,\textsc{iii} are typically blended or
weak; no lines could be detected at all for Feige~48, allowing only
upper limits to be set.

\begin{figure}
\vspace{12cm}
\begin{center}
    \special{psfile=3948fig7a.eps hscale=48 vscale=48 hoffset=10
    voffset=165 angle=360}
    \special{psfile=3948fig7b.eps hscale=48 vscale=48 hoffset=10
    voffset=-10 angle=360}
\end{center}
\caption{Determination of microturbulent velocity of CD~$-24^\circ 731$\ and
  PG~1219$+$534 using Cr\,\textsc{iii} lines. We find
  $\xi=5^{+2}_{-1}$\,km\,s$^{-1}$ for the former, while the latter is
  consistent with $\xi=0$\,km\,s$^{-1}$.}
\label{fig:vmicro}
\end{figure}

\textit{Chromium}: All of our spectra contain many lines of both
Cr\,\textsc{iii} and Cr\,\textsc{iv} of varying strengths. These
lines, along with those of iron, have been used to determine the
microturbulence discussed in Section \ref{sub:micro}.

\textit{Manganese}: Of all the iron-group elements, manganese causes
the largest difficulties, since it appears that many wavelengths given
in the Kurucz list are not accurate (note that the \citet{HH95} list
uses the same wavelengths). We have examined the list of \citet{UR97},
however they only provide improved oscillator strengths, and also use
the Kurucz wavelengths.

\textit{Iron}: In all spectra there are many Fe\,\textsc{iii} and
Fe\,\textsc{iv} lines measurable. In the two hottest objects in our
sample, Fe\,\textsc{v} lines are also present, although
the accuracy of oscillator strengths is uncertain, since the
abundances derived from some of them differ by several orders of magnitude.

\textit{Cobalt}: Lines of Co\,\textsc{iii} and \textsc{iv} are visible
in our spectra, although often only in crowded regions. It appears
that the hotter objects show more strong lines.

\textit{Nickel}: There are very many nickel lines, particularly of
Ni\,\textsc{iii} and \textsc{iv}. A few Ni\,\textsc{v} lines are also
visible in the spectra of PG~1219$+$534\ and Feige~66, however once
again the accuracy of oscillator strengths is very uncertain.

\textit{Copper}: Cu\,\textsc{iii} and \textsc{iv} are both
present. Neither ion is included in the Kurucz list, so wavelengths
were taken from \citet{HH95}. Oscillator strengths are only available
for Cu\,\textsc{iii}. There are no published oscillator strengths of
Cu\,\textsc{iv}.

\textit{Zinc}: Zn\,\textsc{iii} and \textsc{iv} lines are visible;
however, the latter ion has no published oscillator strengths.

\subsubsection{Gallium, Germanium, Tin and Lead}

The discovery of lines of Ga, Ge, Sn and Pb was made by \cite{SJOT04}. Lines
of Ge\,\textsc{iv} and Sn\,\textsc{iv} have also been seen in hot DA white
dwarfs by Vennes, Chayer \& Dupuis (2005).
Abundances for our four targets are almost all done using spectrum synthesis.
Resonance lines of Ga\,\textsc{iii}, Ge\,\textsc{iv}, Sn\,\textsc{iv}, and
Pb\,\textsc{iv} are present in all spectra. In stars with higher Ga
abundances, Ga\,\textsc{iii} subordinate lines are also present. The
resonance line of Sn\,\textsc{iii} at 1251.387\,\AA\ is strong in
Feige~66, and is present in all stars, but is blended.

One of the resonance lines of Pb\,\textsc{iv} is present in each
object; the other line lies in the wings of Ly$\beta$, which is not
covered by our spectra (but is by \emph{FUSE}).

\begin{table*}
\caption{Abundances for each ion for all five targets.}
\label{tab:4abu}
\begin{center}
\begin{tabular}{l||cr|cr|cr|cr|cr}
 & Feige 66 & & PG~1219$+$534\ & & CD~$-24^\circ 731$\ & & Feige 48 & & CPD~$-64^\circ 481$
  & \\
\hline
Ion  &  $\log\epsilon$ & $n$ & $\log\epsilon$ & $n$ & $\log\epsilon$ & $n$ &
$\log\epsilon$ & $n$ & $\log\epsilon$ & $n$ \\
\hline
C\,\textsc{iii} &  6.93$\pm$0.28\rlap{$^*$} &   4 & & & & & 7.22$\pm$0.10 & 3 &
  7.54$\pm$0.22 & 2 \\
C\,\textsc{iv}\rlap{$^*$} & 6.5$\pm$0.5 & 2 & $<$3.1 & & $<$2.7 & &
6.9$\pm$0.5 & & &  \\
N\,\textsc{ii} & & & & & & & & & 7.87$\pm$0.14 & 3 \\
N\,\textsc{iii} &  7.69$\pm$0.23 &   2 & 7.64$\pm$0.42 &  4 & 7.60$\pm$0.47 &
 6 & 7.62$\pm$0.38 & 3 & 7.40$\pm$0.00 & 2 \\
N\,\textsc{iv} & 7.65$\pm$0.00 & 1 & & & & & & \\
N\,\textsc{v}   & 7.60$\pm$0.11 & 2 & 7.58$\pm$0.21 &  2 & 8.26$\pm$0.15 & 2
 & & \\
Al\,\textsc{iii} & $<$3.5 & & $<$3.8 & & $<$3.6 & & 5.51$\pm$0.10 & 3 \\
Si\,\textsc{iii} & & & & & & & 6.43$\pm$0.31 & 8 & 6.38$\pm$0.37 & 3 \\
Si\,\textsc{iv}\rlap{$^*$}  & $<$2.0 & & 3.63$\pm$0.17 &  2 & $<$2.0 & & 6.16$\pm$0.25 &
 3 \\
P\,\textsc{iii} & & & & & & & 4.41$\pm$0.00 & 1 & 4.81$\pm$0.09 & 3 \\
P\,\textsc{iv} & 3.95$\pm$0.00 & 1 & & & & & & \\
S\,\textsc{iii} & 7.69$\pm$0.46 & 4 & 7.00$\pm$0.11 &  3 &
5.7$\pm$0.00 & 1 & & & 6.29$\pm$0.27 & 3 \\
Ar\,\textsc{iii} &  7.86$\pm$0.24 &   4 &  7.02$\pm$0.00 &  1 & $<$7.0
& & $<$7.0 & & & \\
Ca\,\textsc{iii} &  8.09$\pm$0.20 &  20 &  7.73$\pm$0.23 & 10 & 7.50$\pm$0.22
& 8 & 7.31$\pm$0.00 & 1 & 6.97$\pm$0.00 & 1 \\
Sc\,\textsc{iii} & 5.17$\pm$0.51 & 2 & $<$5.0 & & 4.61$\pm$0.00 & 1 & $<$3.0 & & & \\
Ti\,\textsc{iii} &  6.98$\pm$0.22 &   10   &    6.51$\pm$0.20 &  2 &
5.77$\pm$0.06 & 3 & 5.16$\pm$0.20 & 4 & 5.68$\pm$0.37 & 6 \\
Ti\,\textsc{iv}  &  6.91$\pm$0.18 &   5   &    6.73$\pm$0.00 &  1 &
5.87$\pm$0.15 & 3 & 5.21$\pm$0.18 & 2 & 5.75$\pm$0.07 & 2 \\
V\,\textsc{iii} &  6.42$\pm$0.22 &  11   &    5.80$\pm$0.00 &  1  & &
& & & 4.48$\pm$0.15 & 4 \\
V\,\textsc{iv}  &  6.29$\pm$0.14 &   7   &    6.37$\pm$0.34 &  2 &
5.77$\pm$0.37 & 9 & & & & \\
Cr\,\textsc{iii} &  7.29$\pm$0.19 &  65   &    7.23$\pm$0.17 & 44 &
6.96$\pm$0.23 & 44 & 5.90$\pm$0.18 & 29 & 6.20$\pm$0.30 & 33 \\
Cr\,\textsc{iv}  &  7.31$\pm$0.23 &  25	&   7.46$\pm$0.14  & 17 &
7.24$\pm$0.47 & 28 & 6.41$\pm$0.28 & 7 & 6.54$\pm$0.20 & 10 \\
Mn\,\textsc{iii} &  6.02$\pm$0.19 &  12	&   7.25$\pm$0.22 & 46  &
6.89$\pm$0.36  & 19 & 5.62$\pm$0.21 & 13 & 5.54$\pm$0.21 & 15 \\
Mn\,\textsc{iv}  &  5.99$\pm$0.51 &   2	&   7.72$\pm$0.11 &  3  &
7.12$\pm$0.54  & 7 & & & 5.86$\pm$0.18 & 2 \\
Fe\,\textsc{iii} &  6.46$\pm$0.17 &  26	&   7.16$\pm$0.22 & 69  &
6.66$\pm$0.26  & 23 & 7.68$\pm$0.19 & 107 & 7.38$\pm$0.33 & 20 \\
Fe\,\textsc{iv}  &  6.40$\pm$0.10 &  2	&   7.43$\pm$0.22 & 23  &
7.03$\pm$0.25  & 23 & 7.73$\pm$0.21 & 10 & 7.52$\pm$0.23 & 11 \\
Fe\,\textsc{v}   & & & 7.38$\pm$0.41 &  2  & &  & & & & \\
Co\,\textsc{iii} &  6.46$\pm$0.33 &  39 &  6.73$\pm$0.20 & 20  &
6.13$\pm$0.39  & 20 & 5.73$\pm$0.25 & 5 & & \\
Co\,\textsc{iv}  &  6.32$\pm$0.22 &   20 &  6.72$\pm$0.13 & 7  &
6.28$\pm$0.21  & 11 & 6.05$\pm$0.25 & 3 & & \\
Ni\,\textsc{iii} &  6.86$\pm$0.15 &  32 &  7.39$\pm$0.18 & 32  &
6.20$\pm$0.48  & 12 & 6.63$\pm$0.22 & 28 & 6.39$\pm$0.25 & 6 \\
Ni\,\textsc{iv}  & 6.81$\pm$0.25 & 32 &  7.41$\pm$0.27 & 19  & 6.28$\pm$0.28 &
14 & 6.75$\pm$0.21 & 7 & 6.50$\pm$0.26 & 9 \\
Ni\,\textsc{v}   & 6.91$\pm$0.55 & 10 &  7.60$\pm$0.14 & 5  & & & & & & \\
Cu\,\textsc{iii} & 6.27$\pm$0.38 & 8 & 6.36$\pm$0.36 & 5 & & &5.25$\pm$0.40 &
3 & & \\
Zn\,\textsc{iii} &  6.64$\pm$0.35 &   15 &  6.68$\pm$0.36 &  5  &
5.97$\pm$0.50 & 2 & 5.30$\pm$0.22 & 6 & 5.33$\pm$0.34 & 6 \\
Ga\,\textsc{iii} & 5.53$\pm$0.06 & 2 & 5.75$\pm$0.04 & 2 & 5.23$\pm$0.21 & 2 &
4.70$\pm$0.00 & 1 & 3.63$\pm$0.00 & 1 \\
Ge\,\textsc{iv}  & 5.21$\pm$0.05 & 2 & 4.99$\pm$0.03 & 2 & 4.98$\pm$0.01 & 2 &
4.02$\pm$0.08 & 2 & 3.57$\pm$0.10 & 2 \\
Sn\,\textsc{iv}  & 4.12$\pm$0.00 & 1 & 4.08$\pm$0.00 & 1 & 3.11$\pm$0.00 & 1 &
2.94$\pm$0.00 & 1 & 2.86$\pm$0.00 & 1 \\
Pb\,\textsc{iv}  & 4.7$\pm$0.00 & 1 & 4.6$\pm$0.00 & 1 & 4.3$\pm$0.00 & 1 &
3.8$\pm$0.00 & 1 & 3.43$\pm$0.00 & 1 \\
\hline
\end{tabular}
\end{center}
\hspace{2cm}
$^*$Based on non-LTE-affected resonance lines; see Section
\ref{sub:nlte}.
\end{table*}

\section{Abundance analysis}
\label{sec:abu}

\begin{figure}
\vspace{6cm}
\begin{center}
    \special{psfile=3948fig8.eps hscale=50 vscale=50 hoffset=-10 voffset=-10
    angle=0}
\end{center}
\caption{Spectrum fit to the C\,\textsc{iv} resonance lines at 1550\,\AA\ for
  Feige~66. The model is shown as the thick line. The line cores of the model
  do not match the observations, and the abundance is set around 0.8 dex lower
  than that derived from C\,\textsc{iii} lines. See text for details.}
\label{fig:f66c4}
\end{figure}

In this section we comment on results and trends for individual or groups of
elements. The abundances are given in Table \ref{tab:4abu} and plotted
relative to the sun in Figure \ref{fig:4abu}.  The errors
  given were determined using a simple mean and standard deviation
  based on the individual measurement for each line. An error of zero
  represents a measurement taken from only one line. The solar values
were taken from \citet{GS98}. The O, Ne and Mg abundances of the
programme stars are taken from HRW for PG~1219$+$534\ and Feige 48, while for
CD~$-24^\circ 731$\ and CPD~$-64^\circ 481$, they are from Edelmann (private communication), along
with the Al abundance for the latter star.

Before discussing our derived abundances in more detail, however, it
is necessary to first consider non-LTE effects and the effect of
microturbulence on the absorption lines in our spectra.

\subsection{NLTE effects}
\label{sub:nlte}

\begin{figure*}
\vspace{22cm}
\begin{center}
    \special{psfile=3948fig9.eps hscale=98 vscale=98 hoffset=10
      voffset=-60 angle=360}
\end{center}
\caption{Abundances measured for our five targets. Magenta symbols
  represent values determined using singly ionised lines, green
  represents doubly ionised lines, red
  represents triply ionised lines, blue denotes quadruply ionised
  lines and cyan represents upper limits. Note the generally excellent
agreement between different ionisation stages.}
\label{fig:4abu}
\end{figure*}

Most of the spectral lines we are dealing with in this paper are subordinate,
i.e. they are between excited levels and do not involve the ground
level. The
resonance lines (transitions from the ground level) of some ions are present
however, and it is these lines that are most sensitive to departures from our
assumption of local thermodynamic equilibrium (LTE). Ions of
iron-group elements do not appear to be affected, but
species such as C\,\textsc{iv} and Si\,\textsc{iv}, there are noticeable
effects. In Figure \ref{fig:f66c4} we show the C\,\textsc{iv}
resonance lines at 1548\,\AA\ and 1550\,\AA\ of Feige~66 as an
example. In this star and Feige~48 the line cores of these lines are
matched by the abundances derived from the C\,\textsc{iii} lines,
however the wings are much too broad. Reducing the C abundance results
in an improved fit in the wings but a core that is too shallow. This
is most likely a non-LTE effect. Detailed model atom calculations are
needed to confirm this, but are beyond the scope of this paper. There
may also be an interstellar component present, at least in Feige~66,
which has a radial velocity of only $\sim -6$\,km\,s$^{-1}$; however,
this is not the case for Feige~48, and the effect is still present.

In the case of C\,\textsc{iii} all three lines/multiplets can be
matched well with a model spectrum at the listed abundance for
Feige~48, however for Feige~66 things are not so simple. The
1174-1177\,\AA\ multiplet is apparently matched well; the
1247\,\AA\ line is not, while the 2297\,\AA\ line matches in the wings
but not in the line core. Because Feige~66 is around 5000\,K hotter
than Feige~48, we again attribute these problems to non-LTE effects.

The iron-group lines we have used for our abundance analysis are not
resonance lines (with the exception of Ti\,\textsc{iii} where some
resonance lines were used), so are
not likely to be strongly affected by non-LTE effects.

\subsection{Microturbulence}
\label{sub:micro}

Since we have measured the equivalent widths of many lines for several ions,
we can investigate the microturbulence $\xi$ for each star. Both of the
pulsating sdBs, along with CPD~$-64^\circ 481$, are consistent with $\xi=0$\,km\,s$^{-1}$;
however, the two other non-pulsators both have $\xi>0$\,km\,s$^{-1}$. The top
panels of Figure \ref{fig:vmicro} shows the difference between
$\xi=0$\,km\,s$^{-1}$ and the value we derive $\xi=5^{+2}_{-1}$\,km\,s$^{-1}$
for CD~$-24^\circ 731$; the bottom panels show the effect of non-zero microturbulence for
PG~1219$+$534. For Feige~66 we find $\xi=2\pm1$\,km\,s$^{-1}$. These values have been
derived using both Cr\,\textsc{iii} and Fe\,\textsc{iii} lines.

\subsection{Abundances}
\label{sub:comparison}

Before looking at the differences in iron-group abundances of our
targets, we first search for and examine trends amongst the lighter
elements.

\subsubsection{Light metals}

As has been found by many previous studies, carbon abundances range
from virtually none at all to slightly below the solar value. For
PG~1219$+$534\ and CD~$-24^\circ 731$\ the absence of the C\,\textsc{iv} resonance
lines indicates carbon depletion by 10$^5$ or more. Because we cannot
at the moment account for NLTE effects (see \ref{sub:nlte} above)
these have to be regarded as order of magnitude estimates. We note
here that simple NLTE calculations were done by \citet{HHH84} for the
sdO star Feige~110 ($T_{\mathrm{eff}}=40\,000$\,K) and a
similar upper limit was derived.

In the case of nitrogen, the abundances are slightly below the solar
value; this is also in keeping with previous analyses of sdB optical
spectra.  We note in passing that we could not easily fit the
N\,\textsc{iv} line at 1718.551\,\AA\ in all of our sample because of
severe crowding -- only in Feige~66 is the line isolated -- however
the strength of the line is approximately consistent with the
abundances derived from the other N ionisation stages. Note that the
nitrogen abundances from three different ionisation stages are fully
consistent for Feige~66.

For Feige~48 it was not possible to measure the sulfur abundance because the
resonance lines are blended with a large number of metal lines that are not in
the Kurucz list of observed lines or the Hirata \& Horaguchi list. This effect
is seen to a lesser extent in PG~1219$+$534, making a spectrum fit possible,
and hardly seen at all in Feige~66. Because of the absence of heavy crowding
in the latter star, we suggest these may be iron lines. We examined the
effect of including the ``computed'' (but not observed) lines in the Kurucz
list: the match is better for Feige~48, but it is still not possible to
measure abundances using the S\,\textsc{iii} lines.

\subsubsection{Iron group}

As can be seen from Table \ref{tab:4abu}, plenty of lines of doubly
ionised atoms (in particular Cr\,\textsc{iii}, Fe\,\textsc{iii} and
Ni\,\textsc{iii}) have been used for the abundances analysis, for Feige~48
more than 100 Fe\,\textsc{iii} lines were utilised. Moreover, triply
ionised atoms can be used to determine abundances for all iron group
elements as well (except for V\,\textsc{iv} and Mn\,\textsc{iv} in
Feige~48 and V\,\textsc{iv}, and Co\,\textsc{iv} in CPD~$-64^\circ 481$), which in
some stars are also quite numerous (e.g. 32 Ni\,\textsc{iv} lines in
Feige 66). Even four times ionised atoms have been used for analysis
of nickel in Feige~66 and PG~1219$+$534\ and of iron in PG~1219$+$534. It is worthwhile
noting that these ionisation equilibria are very well matched,
e.g. the three ionisation stages of Ni  agree to within 0.1 dex for
Feige 66 and to within 0.2 dex for PG~1219$+$534. For other ions of the iron
group, we find:

\begin{itemize}
\item Fe\,\textsc{iii} and Fe\,\textsc{iv} as well as Ni\,\textsc{iii} and
  Ni\,\textsc{iv}, respectively, agree very well (0.1~dex, typically) for
  Feige~48 and CPD~$-64^\circ 481$\ and to within error limits in CD~$-24^\circ 731$\ (0.37~dex for iron).

\item Cr\,\textsc{iii} and Cr\,\textsc{iv} agree to better than 0.3~dex except
  for Feige~48 (0.5~dex).

\item Mn\,\textsc{iii} and Mn\,\textsc{iv} are in perfect agreement for Feige
  66, differ by about 0.3~dex in CD~$-24^\circ 731$\ and CPD~$-64^\circ 481$. Only for PG~1219$+$534\ they deviate
  beyond the adopted error ranges.

\item Co\,\textsc{iii} and Co\,\textsc{iv} also match very well, to better
  than 0.2~dex, except for Feige~48 which has much less Co lines than the
  other programme stars.

\item Although only few titanium lines could be used for the analysis, the
  results from Ti\,\textsc{iii} and Ti\,\textsc{iv} match extremely
  well for all programme stars.
\end{itemize}

We regard the very good match of many ionisation equilibria as evidence that
systematic errors of the metal abundances and of the effective
temperature are small. This can also be seen in the good match between
synthetic spectrum and observations for three objects shown in Figure
\ref{fig:fe1860}.

While iron is found to be nearly solar (PG~1219$+$534, Feige~48, CPD~$-64^\circ 481$),
slightly depleted in CD~$-24^\circ 731$\ and subsolar in Feige~66 by a factor of ten, all
other elements of the iron group are enhanced by between 0.5 and 2.5 dex with
respect to solar values. The enhancements are large in Feige~66 and PG~1219$+$534, but
mild for the three others.

\begin{figure}
\vspace{6cm}
\begin{center}
    \special{psfile=3948fig10.eps hscale=50 vscale=50 hoffset=-10 voffset=-10
    angle=0}
\end{center}
\caption{Spectrum fit to the Ge\,\textsc{iv} resonance lines at 1189\,\AA\ for
  Feige~66. The model is shown as the thick line. }
\label{fig:f66ge4}
\end{figure}

\subsubsection{Gallium, Germanium, Tin and Lead}

The heavy metals Ga, Ge, Sn and Pb are all enriched with
respect to the Sun in all stars, reaching as high as 2.9~dex for Ga in
PG~1219$+$534\ or 2.75~dex for Pb in Feige~66. An example of a fit of the
Ge\,\textsc{IV} 1189\,\AA\ line is shown in Figure
\ref{fig:f66ge4}. There are several strong lines also present that are
either not identified or have no atomic data. Possible identifications
are shown in the figure.

\subsection{Comparison with previous work}
\label{sub:previous}

As mentioned earlier, many of the objects we have observed for this project
have been studied with optical spectra before -- PG~1219$+$534\ and
  Feige~48 \citep{HRW00}, and CPD~$-64^\circ 481$\ and CD~$-24^\circ 731$\ (Edelmann, private
  communication) -- or with a noisy \emph{IUE} spectrum and poor atomic data
-- Feige~66 \citep{BHS82}. It is useful here to compare our results with these
previous studies, as well as with any general trends seen amongst sdBs as a
group.

Firstly, for the two pulsators PG~1219$+$534\ and Feige~48, our results compare
very well with those of HRW for the limited cross-over that exists
between elements. All of HRW's abundances are, within errors,
consistent with ours, and because we could use resonance lines of
several ions, we have been able to place stronger upper limits on C, Al
and Si for PG~1219$+$534. In the case of
Feige~48 the abundances we derive agree well with those measured by
HRW, and are within $\pm0.04$\,dex.

The only element we have had difficulty
deriving an abundance for is sulfur, for the reasons discussed earlier.

In the case of Feige~66, \citet{BHS82} used \emph{IUE} spectra with
lower resolution than ours, and obtained somewhat different results to
ours. It is difficult to compare the two sets of abundances since
\citeauthor{BHS82} do not give error estimates explicitly; however, if
we assume the same errors as those given for another sdB, HD\,149382,
in the same paper, our values are not so discrepant after all. At the
time of \citeauthor{BHS82} study, the quality of atomic data was lower
than it is at present (although in many cases it is still insufficient
or of low accuracy), so their errors are very large, particularly for
the iron group.

Recently, \citet{EHN06} has carried out an analysis
of CPD~$-64^\circ 481$\ and CD~$-24^\circ 731$\ based on high-resolution optical echelle
spectra. For both stars their abundances are consistent with
those determined here.

Finally, we can also compare any apparent trends seen here with the work of
\citet{HE04}, especially for the lighter elements plus iron.
Both our results here and the work of \citet{HE04} suggests that aluminum
follows the same trend as silicon.

\subsection{Heavy element abundance trends?}
\label{sub:fetrend}

\begin{figure}
\vspace{7.5cm}
\begin{center}
    \special{psfile=3948fig11.eps hscale=53 vscale=53 hoffset=10
    voffset=-10 angle=360}
\end{center}
\caption{Trends in heavy element abundances with iron abundance.}
\label{fig:fetrend}
\end{figure}

An interesting result not immediately obvious from the abundances in Table
\ref{tab:4abu} is a possible anti-correlation between heavy element abundance
and iron abundance. The spread in iron abundance is 1.25 dex from the most
iron-poor (Feige~66) to the most iron-rich star (Feige~48), while the variation
(X/Fe) is between 2 and 3 dex (except for Mn and Ni). Therefore this trend
does not simply reflect the trend in iron abundance.
Four examples of this effect are
shown in Figure \ref{fig:fetrend} for Ca/Fe, Ti/Fe, Ni/Fe and Pb/Fe while
Table \ref{tab:fetrend} shows data for all elements; where there are two or
more ionisation stages, a weighted average is presented. The same basic trend
is seen for all elements in the iron-group, except for manganese and perhaps
nickel, and it is also seen for the heavier elements gallium, germanium, tin
and lead. Caution must
be applied here however, since we have only five objects in our sample. A more
detailed analysis may be possible for at least titanium, since several sdB
stars show Ti\,\textsc{iii} lines in their optical spectra (H. Edelmann,
C. Karl, private communication). If these trends are real we believe they are
caused by a combination of radiative levitation, gravitational settling and a
weak stellar wind, and therefore would help constrain diffusion models. We
urge more theoretical work in this area.

\begin{table}
\caption{Average iron abundance and ratio of heavy element abundances to iron
  for the five targets stars. The columns are as follows: F66 = Feige~66; CD =
  CD~$-24^\circ 731$; PG = PG~1219$+$534; CPD = CPD~$-64^\circ 481$; F48 = Feige~48. Abbreviations: n-v = non-variable,
  var. = variable.}
\label{tab:fetrend}
\begin{center}
\begin{tabular}{l|rrr|rr}
 & F66 & CD & PG & CPD & F48 \\
 & n-v & n-v & var. & n-v & var\\
\hline
Fe & 6.46 & 6.85 & 7.23 & 7.43 & 7.68 \\
\hline
Ca/Fe & 1.63    & 0.65    & 0.50     &  $-$0.46  &  $-$0.37 \\
Ti/Fe & 0.50    & $-$1.03 & $-$0.65  &  $-$1.74  &  $-$2.50\\
V/Fe  & $-$0.09 & $-$1.08 & $-$1.08  &  $-$2.95  &   ---   \\
Cr/Fe & 0.84    & 0.23    & 0.06     &  $-$1.15  &  $-$1.68 \\
Mn/Fe & $-$0.44 & 0.10    & 0.05     &  $-$1.85  & $-$2.06 \\
Co/Fe & $-$0.05 & $-$0.69 & $-$0.50  &    ---    & $-$1.83 \\
Ni/Fe & 0.39    & $-$0.61 & $-$0.19  &  $-$0.97  & $-$1.03 \\
Cu/Fe & $-$0.19 &  ---    & $-$0.87  &    ---    & $-$2.43\\
Zn/Fe & 0.18    & $-$0.88 & $-$0.59  &  $-$2.10  & $-$2.38\\
Ga/Fe & $-$0.93 & $-$1.62 & $-$1.70  &  $-$3.80  & $-$2.98 \\
Ge/Fe & $-$1.25 & $-$1.87 & $-$2.02  &  $-$3.86  & $-$3.66\\
Sn/Fe & $-$2.34 & $-$3.74 & $-$3.11  &  $-$4.57  & $-$4.74 \\
Pb/Fe & $-$1.76 & $-$2.55 & $-$2.53  &  $-$4.00  & $-$3.88 \\
\hline
\end{tabular}
\end{center}
\end{table}

\subsection{Comparison of abundances of pulsator/non-pulsator pairs}
\label{sub:pnpcomp}

 The results of our spectral analysis
allow us to compare the abundance
patterns of four pairs of stars, having similar effective temperature:
(i) the ``cool'' pulsator/non-pulsator pair Feige~48/CPD~$-64^\circ 481$,
(ii) the ``hot'' pulsator/non-pulsator
pair PG~1219$+$534/CD~$-24^\circ 731$, (iii) the ``hot'' pulsator/non-pulsator pair PG~1219$+$534/Feige~66 and
(iv) the pair of
two ``hot'' non-pulsators Feige~66/CD~$-24^\circ 731$.
 We plot the relative iron group abundances for all four combinations
in Fig.~\ref{fig:ironcomp}).

(i) If we compare Feige~48
and CPD~$-64^\circ 481$\ (the bottom panel of Figure \ref{fig:ironcomp}), we
find basically no difference. Not only are the abundances of
the iron group elements similar, but the lighter and
heavier elements also agree reasonably well.
The only exception is gallium which is ten times higher in Feige~48 than in
CPD~$-64^\circ 481$.  Also looking at abundance ratios of iron group elements
with respect to iron (X/Fe, Table \ref{tab:fetrend}) reveals, that the
patterns for Feige~48 and CPD~$-64^\circ 481$\ match each other reasonably well.
This would indicate that there
is no difference in iron group abundances of a pulsator and a non-pulsator.

(ii) The comparison of ``hot'' pulsator PG~1219$+$534\ to the non-pulsator CD~$-24^\circ 731$\ reveals
large differences for some light elements, silicon and sulphur being much
less in CD~$-24^\circ 731$\ (more than 1.6 dex and 1.3 dex, respectively). Significant
differences are also detected for the iron group as well as for the
heavy elements. They, however, vanish almost if the difference in iron
content is accounted for (except for Ni/Fe and Sn/Fe, see
Table~\ref{tab:fetrend}). Since the iron group elements
are probably the drivers for pulsators, the comparison would indicate as in
the previous case that there is little difference (if at all) between
a pulsator and a non-pulsator.

(iii) The comparison of the ``hot'' pulsator PG~1219$+$534\ to the non-pulsator Feige~66
yields a completely different picture. Abundances of several iron group elements
differ (see Table~\ref{tab:4abu}). Even if we take into account the large
difference in iron abundance (factor of 7) between the two stars, the
abundance patterns remain dissimilar (see Table~\ref{tab:fetrend}). Amongst the
light elements there is a huge difference in carbon
abundance. PG~1219$+$534\ has less than 5000 times as much C as Feige~66
has. The abundances of the heavy elements (Ga, Ge,
Sn, and Pb), however, are quite similar. In contrast to the previous comparisons
in (i) and (ii) this would imply that indeed pulsators and non-pulsators have
\emph{different} iron group abundances.

(iv) The comparison of the two ``hot'' non-pulsators Feige~66 and CD~$-24^\circ 731$\ also
reveals large differences in the abundances of iron group elements which
persist if we account for the different iron abundance
(see Table~\ref{tab:fetrend}). Amongst the light elements as well as among the
heavy elements there are large differences as well, which persist if we account for the
different iron abundances.

The last finding is discouraging. If the difference among non-variable
stars of similar $T_{\mathrm{eff}}$ and  $\log g$ are as large as we observe,
the comparison between a pulsator and a non-pulsator is rendered arbitrary.

\begin{figure}
\vspace{11.5cm}
\begin{center}
    \special{psfile=3948fig12.eps hscale=50 vscale=50 hoffset=0
    voffset=-30 angle=360}
\end{center}
\caption{Comparison of iron-group abundances for our
  pulsator/non-pulsator pairs (F48\,=\,Feige~48; CPD\,=\,CPD~$-64^\circ 481$;
  PG\,=\,PG~1219$+$534;
  CD\,=\,CD~$-24^\circ 731$; F66\,=\,Feige~66). The dotted lines denote
  equal abundances and the difference in iron abundance. The
  differences between  PG~1219$+$534, CD~$-24^\circ 731$\ and Feige~66 are quite large
  -- particularly for Fe, Ni and Mn -- while the pairs
  PG~1219$+$534\ $\&$ CD~$-24^\circ 731$\ and Feige~48 $\&$ CPD~$-64^\circ 481$\ show
  quite similar abundances, in particular when the differences in iron abundance
  are accounted for (see text).}
\label{fig:ironcomp}
\end{figure}

The theory of \citet{CFB97a} does not specifically rule out iron-group
elements other than iron itself as responsible for pulsation
driving. In particular Ni must be considered as it has substantially
more UV and FUV lines than iron. Indeed, in the case of PG~1219$+$534\ the nickel
abundance is high
enough that it could make a significant contribution to the opacity,
at least as much as iron. When we consider Feige~48 and CPD~$-64^\circ 481$, we find
that perhaps the difference in the \emph{combined} opacity of iron and
nickel between the two stars is significant enough to discriminate
between pulsator and non-pulsator. This leads us to ask: could we
theoretically have a pulsator with lower iron, but much higher
nickel or other iron-group abundance than a non-pulsator?

\section{Further discussion}
\label{sec:disc}

As seen in Section \ref{sub:tempfix}, enhanced metal abundances can
have an effect on $T_{\mathrm{eff}}$ and $\log g$ determination,
especially for stars showing both neutral and singly ionised
helium. It is also clear that simply scaling models from solar
metalicity ODFs is insufficient; opacity sampling is required for more
accurate measurements, since while Fe abundances are approximately
solar, elements such as Ni and Mn -- which have a significant opacity
contribution -- are almost always enhanced. A preliminary study has
been done in this direction by \citet{BJ06} and \citet{PNE06}.

The effect of these abundance patterns may be apparent for atmosphere
models, but what about stellar evolution and pulsation models? We urge
evolution theorists to investigate the effect of non-solar opacity
distributions on hot subdwarf evolution. In a similar vein, interior models
that include differential internal rotation and/or magnetic fields should also
investigate their effect on diffusion.

In a study of elements beyond the iron group in hot subdwarfs,
\citet{SJOT04} proposed a solution to  the silicon problem discussed in
Section 4.3.2. Triply ionised elements of the same group in the
Periodic Table as silicon -- germanium, tin and lead -- are present in
almost all sdB spectra at \emph{all} temperatures. Si\,\textsc{iv} on the
other hand, almost completely disappears above 32\,000\,K. This shows
that arguments where silicon is ionised to  nobe gas configuration,
i.e. to Si\,\textsc{v}, and then
sinks deeper into the atmosphere, cannot be correct. If this were the
case, these heavier elements, which should feel the same  low radiative
forces as silicon, should also sink. Instead, \citet{SJOT04} suggested
that above $\sim$32\,000\,K silicon could be carried away by a weak
fractionated stellar wind, whereas the heavier elements should stay
behind. Indeed, \citet{Unglaub06} has found that a one-component,
uniform wind is inconsistent with observations, and that multicomponent
calculations are required, although this depends on
  surface gravity and mass-loss rate. When we examine the abundances
of Ge, Sn and Pb, we find that they are all higher in the hot stars
(Feige~66, CD~$-24^\circ 731$, and PG~1219$+$534) that show little or no silicon, than in the
cooler stars (Feige~48, CPD~$-64^\circ 481$) that do. This is what one would
qualitatively expect from the hypothesis of \citet{SJOT04}. Using
\emph{FUSE} spectra, \citet{CFF06} found many other sdBs with similar
properties, but also some exceptions. The case of C\,\textsc{iv} is
not at all straightforward, since it is very difficult to explain two
spectroscopically similar stars, one with measureable silicon but no
carbon (PG~1219$+$534), and the other with measureable carbon but no silicon
(Feige~66). CD~$-24^\circ 731$\ has no carbon and no silicon, compounding the
problem. The reason for this remains a mystery, and presents
  a challenge to the fractionated wind hypothesis, especially since
  carbon is also in the same group as silicon, germanium, tin and
  lead, and should in principle feel the same radiative forces.

It is also worth noting that PG~1219$+$534, one of our pulsators, shows measurable
traces of silicon, despite being hotter than 32\,000\,K, while the
spectroscopically similar  stars Feige 66 and CD~$-24^\circ 731$\ do not. Could
this be an indicator of the age of the sdB? If the star has a weak
fractionated wind, as suggested by \citet{SJOT04}, then perhaps one of
the differences between PG~1219$+$534\ and Feige~66/CD~$-24^\circ 731$\ is age. In order to
determine this, however, diffusion models including silicon are required.

It seems clear that radiative acceleration is bringing heavy elements to the
surface in these sdBs, and perhaps even expelling them through a stellar
wind. We can at least qualitatively understand this in the case of the
iron-group and heavier elements: in the hotter stars heavy elements are much
more enhanced than in the cooler stars. We must also consider, however, that
two of our ``hot'' stars are apparently single, while both of our ``cool''
stars are in close binary systems. Does this have any effect on the
abundance patterns?
It is unclear what the cause
for the differences  among the ``hot'' stars, Feige~66, CD~$-24^\circ 731$, and PG~1219$+$534, is,
but binarity is one possibility.
Our small
number statistic  is the main limiting factor for this discussion, so we must
look forward to the abundance analyses of Edelmann et al. (2006), who
have studied a larger number of binaries and single stars,
albeit with optical spectra, which restricts the available heavier
elements to iron and sometimes titanium.

\section{Summary and Conclusions}
\label{sec:conc}

We have analysed high-resolution UV echelle spectra of five hot
subdwarf B stars, two of which are member of the short-period, pulsating
V361\,Hya class.
 Abundances of no less than 25 elements including the iron group and
  even
  heavier elements such as tin and lead have been determined using
  LTE curve-of-growth and spectrum
  synthesis techniques.
  Our investigation was initiated to test the hypothesis that a
correlation exists between the abundances of iron-group elements in
sdB stars and pulsation. We have compared a hot pulsator (PG~1219$+$534) with a
 two non-pulsators with similar stellar parameters (Feige~66 and CD~$-24^\circ 731$)
and a cooler pulsator
(Feige~48) with a similar non-pulsator (CPD~$-64^\circ 481$), and found no consistent
differences between the members of each pair.
 The heavy element abundance pattern of CD~$-24^\circ 731$\ comes close to that
observed for PG~1219$+$534\ except for its low iron and nickel. Feige~66 has an even lower
iron abundance, but its heavy metal abundance pattern does not match that of
PG~1219$+$534\ at all. In other words the abundance patterns of two non-variable stars
of similar temperature and gravity are too dissimilar for a conclusive
comparison with a pulsator. This result
leads us to suspect
that there must be another, as yet unknown, discriminating factor between
pulsating and non-pulsating sdB stars.

More generally, we have uncovered a potential solution to the discrepant
effective temperatures from Balmer lines and helium ionisation equilibria,
with a significant improvement found using supersolar metallicity
models. Opacity sampling in place of distribution functions will sure lead to
all model line profiles matching observations. Additionally, our spectra show
light element abundance patterns typical for sdBs: carbon varies from
virtually none to around 1 dex below solar, while nitrogen is within 0.5 dex
of the solar value. There is evidence to support the fractionated weak stellar
wind hypothesis of \citet{SJOT04}, as the heavy element abundances increase
with temperature. We also find an interesting anti-correlation between the
abundance of iron and the heavy element abundance relative to iron. More
observations are needed to confirm this trend.

So somewhat frustratingly we must conclude that we cannot provide any
insights into pulsation in sdB stars based on our spectroscopic
measurements. On a more encouraging note, the results presented here will
provide a valuable resource for theoretical work into diffusion in sdB
stars. It will be important to study the diffusion of all iron group
and heavier elements individually in order to explain the trend we
have uncovered. We end then with a question and a challenge: how can we
find the reason some sdB pulsate and some don't if not by
spectroscopic means?

\begin{acknowledgements}
We thank the referee for constructive comments that have improved the
manuscript. We would like to thank  Michael Lemke for his support with the
LINFOR code and Norbert Przybilla for useful
discussions on the quality of atomic data. SJOT is supported by the
Deutsches Zentrum f\"ur Luft- und Raumfahrt (DLR) through grant
no.\ 50-OR-0202.
\end{acknowledgements}

\bibliographystyle{aa}

redpajama_set_name: RedPajamaArXiv


text:
Q: End Point Not found in WCF Restful Service I am creating a sample wcf service to test with one of my client.
I am getting result using SOAP, But REST is not working. It shows "Endpoint Not Found" error.
Here is my Web.Config for WCF service. Can anybody tells me what's wrong with this config file.
 <?xml version="1.0"?>
 <configuration>
<appSettings>
<add key="aspnet:UseTaskFriendlySynchronizationContext" value="true" />
</appSettings>
<system.web>
<compilation debug="true" targetFramework="4.5" />
<httpRuntime targetFramework="4.5"/>
 </system.web>
 <system.serviceModel>
 <behaviors>
  <serviceBehaviors>
    <behavior name="web">
      <!-- To avoid disclosing metadata information, set the values below to false before deployment -->
      <serviceMetadata httpGetEnabled="true" httpsGetEnabled="true"/>
      <!-- To receive exception details in faults for debugging purposes, set the value below to true.  Set to false before deployment to avoid disclosing exception information -->
      <serviceDebug includeExceptionDetailInFaults="false"/>
    </behavior>
  </serviceBehaviors>
<endpointBehaviors>
  <behavior name="restbehavior">
    <webHttp/>
  </behavior>
</endpointBehaviors>
</behaviors>

<services>
  <service name ="s2HCloudService.Service1"
  behaviorConfiguration="web" >

    <endpoint name ="SOAPEndPoint"
    contract ="s2HCloudService.IService1"
    binding ="basicHttpBinding"
    address ="soap" />

    <endpoint name ="RESTEndPoint"
    contract ="s2HCloudService.IService1"
    binding ="webHttpBinding"
    address ="rest"
    behaviorConfiguration ="restbehavior"/>

    <endpoint contract="IMetadataExchange"
    binding="mexHttpBinding"
    address="mex" />
  </service>
</services>

<protocolMapping>
    <add binding="basicHttpsBinding" scheme="https" />
   </protocolMapping>
   <serviceHostingEnvironment aspNetCompatibilityEnabled="true" multipleSiteBindingsEnabled="true" />
  </system.serviceModel>
  <system.webServer>
  <modules runAllManagedModulesForAllRequests="true"/>
  <!--
    To browse web app root directory during debugging, set the value below to true.
    Set to false before deployment to avoid disclosing web app folder information.
-->
   <directoryBrowse enabled="true"/>
  </system.webServer>

 </configuration>

redpajama_set_name: RedPajamaStackExchange


text:
Q: C++ compile issues Hello I am getting compile errors and I don't understand why

*

*2   IntelliSense: expected an identifier    c:\Users\Sean\Documents\Visual Studio 2013\Projects\mystring\mystring\mystring.cpp  93  7   mystring

*3   IntelliSense: expected a ';'    c:\Users\Sean\Documents\Visual Studio 2013\Projects\mystring\mystring\mystring.cpp  93  10  mystring

*4   IntelliSense: member function "main_savitch_4::mystring::operator=" may not be redeclared outside its class c:\Users\Sean\Documents\Visual Studio 2013\Projects\mystring\mystring\mystring.cpp  106 17  mystring

*5   IntelliSense: expected a ';'    c:\Users\Sean\Documents\Visual Studio 2013\Projects\mystring\mystring\mystring.cpp  107 2   mystring

*6   IntelliSense: more than one operator ">>" matches these operands:
        function "operator>>(std::istream &ins, main_savitch_4::mystring &target)"
        function "main_savitch_4::operator>>(std::istream &ins, main_savitch_4::mystring &target)"
        operand types are: std::istream >> main_savitch_4::mystring c:\Users\Sean\Documents\Visual Studio 2013\Projects\mystring\mystring\mystring.cpp  246 7   mystring
#include <iostream>
#include "mystring.h"
#include <cstring>
using namespace std;
using namespace main_savitch_4;

//Constructors- sets initial values for memeber variables

  mystring::mystring(const char str[] = "")

//returns a pointer referencing [0] in an array
{
current_length = 0;
int pt = 0;

if (str[pt] != '\0') //this increases the array size to the string size
{
    ++current_length;
    ++pt;
}

sequence = new char[current_length + 1];
while (current_length >= pt)
{
    sequence[pt] = str[pt];
    ++pt;
}
allocated = current_length + 1;
}

mystring::mystring(const mystring& source)
{
sequence = new char[source.allocated];
current_length = source.current_length; //returns mystring object with same
allocated = source.allocated;           //length and allocation as source
for (int i = 0; i <= allocated; ++i)
{
    sequence[i] = source.sequence[i]; //copies characters to new object
}

}

//Destructor- frees space
mystring::~mystring()
{
        delete[] sequence;
}

void mystring::operator +=(const mystring& addend)//adds another string ontop of the original
{

reserve(current_length + addend.current_length + 1);
strcpy(sequence + current_length, addend.sequence);
current_length += addend.current_length;
}
    void mystring::operator +=(const char addend[])
    {
int leng = current_length + strlen(addend);
if (leng >= allocated)
        {
    reserve(leng + 1);
}

strcpy(sequence + current_length, addend);
current_length = leng;
}

void mystring::operator +=(char addend)
{
while (current_length >= allocated)
{
    reserve(current_length + 1);
}

sequence[current_length] = addend;
sequence[current_length + 1] = '\0'; //increases size to allow for \0     character
++current_length;

        }

 void mystring::reserve(size_t n) //size_t represents the size of object
// n is the size

{

    if (allocated < n)
    {

    char[] sequence = new char[n];
    for (int i = 0; i <= current_length; ++i)
    {
        sequence + i;
        allocated = n;
    }

}

/////////////////////

void mystring::operator =(const mystring& source)
{

    delete[] sequence;
    sequence = new char[source.allocated];
    allocated = source.allocated;
    current_length = source.current_length;

    for (int idx = 0; idx <= source.allocated; ++idx)
    {
        sequence[idx] = source.sequence[idx];
    }

}

char mystring::operator [ ](size_t position) const

{
    return sequence[position];
}

std::ostream& operator <<(std::ostream& outs, const mystring& source)

{
    outs << source.sequence;

    return outs;
}

bool operator ==(const mystring& s1, const mystring& s2)

{
    int length = 0;
    bool gate = false;

    if (s1.length() >= s2.length())
        length = s1.length();
    else
        length = s2.length();

    for (int idx = 0; idx < length; ++idx)
    {
        if (s1[idx] - s2[idx] == 0 && idx == length - 1)
            gate = true;
    }

    return gate;
}

bool operator !=(const mystring& s1, const mystring& s2)

{
    return !(s1 == s2);
}

bool operator >=(const mystring& s1, const mystring& s2)

{
    if (s1 < s2)
        return false;
    else
        return true;
}

bool operator <=(const mystring& s1, const mystring& s2)

{
    if (s1 > s2)
        return false;
    else
        return true;
}

bool operator > (const mystring& s1, const mystring& s2)

{
    bool gate = false;
    int length = 0;

    if (s1.length() <= s2.length())
        length = s1.length();
    else if (s1.length() > s2.length())
        length = s2.length();

    for (int idx = 0; idx < length; ++idx)
    {
        if (s1[idx] - s2[idx] < 0)
        {
            gate = true;
            idx = length;
        }
        else if (idx == length - 1 && s1.length() < s2.length())
        {
            gate = true;
        }
    }

    return gate;
}

bool operator < (const mystring& s1, const mystring& s2)

{
    if (s1 != s2 && s2 > s1)
        return true;
    return false;
}

mystring operator +(const mystring& s1, const mystring& s2)

{
    mystring temp(s1);
    temp += s2;
    return temp;
}

std::istream& operator >>(std::istream& ins, mystring& target)

{
    while (ins && isspace(ins.peek()))
    {
        ins.ignore();
    }

    target = ""; //Clear out any junk in the target

    while (ins.peek() != '\n')
        target += ins.get();

    return ins;
}

std::istream& getline(std::istream& ins, mystring& target)

{
    ins >> target;

    return ins;
}

A: This if statement in function reserve:
void mystring::reserve(size_t n)
{
    if (allocated < n)
    {

    char[] sequence = new char[n];
    for (int i = 0; i <= current_length; ++i)
    {
        sequence + i;
        allocated = n;
    }
}

Doesn't appear to be closed. Try adding a }.


text:
Martin De Prycker (b. Sint-Niklaas, 16 January 1955) is a Belgian engineer and businessman. He was until December 2008 the CEO of Barco, a Belgian display hardware manufacturer. He currently serves as CEO of Caliopa, a spin-off of Ghent University and IMEC and is managing partner at Qbic fund.

Education
He graduated as a MSc in electrical engineering (1979) and holds a PhD in computer sciences (1982) from Ghent University. In addition, he obtained an MBA at the University of Antwerp in 1992.

Career
He started his career at Alcatel in 1982, at that time ITT. During his career at Alcatel, he held various key positions in Alcatel's research center in Antwerp. In 1985, he started research on ATM, which resulted in a first world prototype in Telecom Geneva in 1991. In 1996, as head of the Access Business Unit, he led Alcatel's ADSL virtual company for the development of ADSL. In 2000, he became Chief Technology Officer (CTO) and a member of the executive committee of Alcatel in Paris. In February 2002, he became the CEO of Barco, where he succeeded Hugo Vandamme.

Martin De Prycker was teaching at Boston University from 1988 to 1992 and at Ghent University from 1994 to 1999.

He is a member of the board of Agoria and of VOKA. In addition he is a member of the committee  of the Flemish Council for Science Policy and of the board of advice of the GIMV.

Bibliography
 Martin De Prycker, Asynchronous Transfer Mode: Solution for the Broadband ISDN, Prentice Hall PTR; 3Rev Ed edition (23 August 1995),

Sources

 Martin De Prycker wordt nieuwe CEO van BARCO (press release)
 Martin De Prycker wordt nieuwe CEO van BARCO

1955 births
Living people
Belgian businesspeople
Ghent University alumni
People from Sint-Niklaas

redpajama_set_name: RedPajamaWikipedia


We need to keep positive and play on the front foot and surely results will become in our favour.
Last night left us shaking our heads in disbelieve .
Last edited by STAGS FOR LIFE on Wed Oct 03, 2018 12:15 pm, edited 1 time in total.
Shakers 0-2 Stags. It's coming together.
I reckon it's gonna be tough, tougher than last night without a doubt. However if we play as well as last night Bury will be chasing shadows. All that then remains is for us to score.
That's funny, I thought we had Mr Oldham on Tuesday night.
Spiritater wrote: I reckon it's gonna be tough, tougher than last night without a doubt. However if we play as well as last night Bury will be chasing shadows. All that then remains is for us to score.
Frustrating as it'd be that's probably be the biggest compliment they could give us.
I think they'll be pushing hard to come back from home defeat to Carlisle, so head says 1-1.
Depends if we can take our chances.
Is 2 nil win too optimistic?
Despite being impressed with us on Tuesday i think we might struggle today. Fingers crossed we can play like we did and take the game to them.
Unfortunately, I predict another depressing result in Flitcroft's reign. Please don't play one upfront!
Two good footballing sides but Bury to win 2-0.
An interesting debate on Flickers (not flip flop) on Bury's forum.
three different stags players slipped in the first 90 seconds.


text:
Home » Prince George's County, MD News » Some Prince George's school…
Some Prince George's school board members want Skins to tap Kaepernick
Melissa Howell | mhowell@wtop.com
Some school board members in Prince George's County are standing behind NFL quarterback Colin Kaepernick, urging the Washington Redskins to give him a chance to get back in the game.
WASHINGTON — Some school board members in Prince George's County are standing behind NFL quarterback Colin Kaepernick, urging the Washington Redskins to give him a chance to get back in the game.
Seven of the 14 Prince George's County School Board members expressed support for Colin Kaepernick not just on the field but as a community leader, in a letter sent to the Washington Redskins on Thursday.
As the Redskins deal with multiple injuries among players, several board members are asking the team to give Kaepernick an immediate tryout and wrote:
"Giving Kaepernick an opportunity would send an even more powerful message today to our community and our students; that a person can peacefully protest for causes that they believe in and not be punished for it even though they are otherwise qualified for the position."
Column: Redskins unwittingly prove Kaepernick's worth
Kaepernick hasn't played in the NFL since 2016, when he protested police brutality and racial injustice against African-Americans by kneeling during the national anthem, a move that's sparked debate on both sides.
FedEx Field, where the Redskins play, is in Prince George's County.
Read the open letter, a copy of which was sent to WTOP, below:
Dear Daniel Snyder, Bruce Allen, and Doug Williams,
We'd like to first thank you for the charitable work that your franchise has done and is still doing for Prince George's County Public Schools. As a school system, we pride ourselves on our ability to prepare our students to take full advantage of all the opportunities available to them. We write you today about a matter that's on the minds of many Prince Georgians, as well as fans nationwide. Our view is that the Washington Football Team needs to give Colin Kaepernick an opportunity to join the team in a form of a try-out, and need to do so immediately.
Our reasoning goes far beyond football. While it is apparent that Kaepernick is at least deserving of a roster spot based on his track record as an NFL quarterback, we think he merits an opportunity for other reasons. Historically this organization shown leadership in the National Football League. As you know in 1987 Doug Williams became the first black quarterback to lead an NFL team to a [Super Bowl] victory. For African-American boys around America and especially here in the DC area, one didn't have to look far for inspiration.
Fast forward 30 years, and the need for this franchise to lead the NFL is still there. Giving Kaepernick an opportunity would send an even more powerful message today to our community and our students; that a person can peacefully protest for causes that they believe in and not be punished for it even though they are otherwise qualified for the position.
As school board members our reasons for wanting Kaepernick to get a try-out are simple. We believe that giving Kaepernick an opportunity will send the right message to our students and community members, who see him as someone who cares about issues affecting our community. If signed, we look forward to working with him, and the Washington organization to create the types of programming and spaces for our young people to discuss and debate the issues affecting them. If Kaepernick is signed we hope to work with his philanthropic organization to partner with our most needy students and provide more opportunities for our students.
As school board members, not standing for the national anthem wouldn't cost us the opportunity to work, and it shouldn't cost him either.
We look forward to hearing from you, and getting this done for the benefit of Prince Georgians and Redskins fans everywhere. We know that this decision is not an easy one and that there could be backlash. We stand ready to support you in doing the right thing and making a decision that will help the team and our community on and off the field.
David Murray, Board Member, District 1
Joshua M. Thomas, Board Member, District 2
Belinda Queen, Board Member, District 6
Edward Burroughs, III, Board Member, District 8
Amanya Paige, Student Board Member
Curtis Valentine, Board Member, At Large
Paul Monteiro, Board Member, At Large
WTOP's Will Vitka contributed to this report.
Luke Garrett
Luke Garrett is a D.C. native dedicated to journalism. He is the co-creator, host and producer of the original WTOP podcast, "Is It Normal Yet?!" The podcast debuted in 2021 and takes a weekly look at how the D.C. region is dealing with coronavirus.
lgarrett@wtop.com
@lukegarrett202
Local News | Maryland News | NFL News | Prince George's County, MD News | Sports | Washington Commanders | Washington, DC Sports
Colin Kaepernick | Melissa Howell | quarterback | schools
Like WTOP on Facebook and follow @WTOP on Twitter to engage in conversation about this article and others.
© 2018 WTOP. All Rights Reserved. This website is not intended for users located within the European Economic Area.

redpajama_set_name: RedPajamaCommonCrawl


text:
How to Increase Reception on a Motorola RAZR
How to Set Up a Laptop With a Projector
How to Boost Handheld Scanner Radio Frequency
by Fred Decker
What Is the Problem if There's Static in My Computer Headphones?
How to Stop the Shaking of a Mounted Projector
What Do You Need to Attach a Monitor to a Laptop?
How to Install a Network for Windows XP Service Pack 2
Radio-frequency scanners are an absorbing hobby for enthusiasts, but they're also a useful tool in many lines of business. Your radio system's base unit can monitor your crews in the field, but it's not portable. With a handheld scanner, you can keep track of your team from your desk, your car, or a different jobsite. The flexible antenna that came with your handheld will receive most frequencies adequately, but, for some, you might need a better antenna.
Upgrade Your Antenna
Check with your technical staff to verify which frequencies you need to receive. Antennas are designed to receive varying bands, and buying one that doesn't receive your frequencies will be of little help.
Replace the flexible "rubber duck" antenna that came with your scanner. They usually attach with a standard push-and-twist BNC connector. Twist the original antenna to remove it, and replace it with a telescoping steel antenna. Raise and lower the antenna until you find the length that gives you the best reception in your troublesome frequencies. You can use this antenna anywhere.
Place a magnet-mount scanner antenna on your car or work vehicle so that you can monitor frequencies more effectively while you're on the road. Be sure to purchase a car antenna that receives the frequencies with which you are having trouble.
Install an outdoor antenna on your building. Some are omnidirectional, and will pick up transmissions from all around your location. Others provide a stronger signal but only do so in one direction. This can be your best option if your crews work in a relatively narrow area, or if your location is on the outskirts of your town or city.
If your scanner simply isn't capable of receiving a specific band of frequencies, the simplest answer is to buy a new scanner that will. However, you might be able to purchase or build a frequency converter that will receive the necessary band and convert it down to one that your scanner receives well. This requires some fairly advanced DIY skills, but, if there's an active ham radio club in your area, you might be able to have them custom-build one for you. Converters are sometimes available from online radio-products dealers.
RadioShack: Scanner Frequently Asked Questions
Long Island Area Scanning Resources: Guide to Scanner Antennas
Fred Decker is a trained chef and certified food-safety trainer. Decker wrote for the Saint John, New Brunswick Telegraph-Journal, and has been published in Canada's Hospitality and Foodservice magazine. He's held positions selling computers, insurance and mutual funds, and was educated at Memorial University of Newfoundland and the Northern Alberta Institute of Technology.
How to Connect an iPod to an LCD Projector
Why Does My Wireless Keyboard Miss Keystrokes?
How to Hang an Overhead Projector
How to Improve Cell Phone Reception in a Concrete Building


The National Weather Service at State College has issued a frost advisory for York County beginning at 1 a.m. and continuing until 9 a.m. Monday, Oct. 22.
According to the advisory, temperatures will be in the low- to mid-30s and could damage "sensitive vegetation." Potted plants should be brought indoors.
Meteorologists at NWS State College predict sunny skies and a high of 54 degrees Monday.


Researchers come up with a mathematical ratio for beauty, how do you measure up?
Researchers, who probably get paid a lot to figure these things out, have used a variety of experiments to determine what goes into a beautiful face. Using Photoshop, they kept eyes, mouth, nose, contour, and hair features the same, but changed the vertical and horizontal distances between them and then asked subject to judge which pictures were more attractive. Vertically, the ideal distance between the eyes and mouth as compared to total face length, measured from the hairline to the chin is 36. Horizontally, having the distance of the eyes is 46 percent of the total face width was found to be the magic number. Fortunately, the 36/46 ratios are those of an average face. And even if your numbers aren't perfect, having the right haircut can alter your ratio to fit. Don't have the right ratio? No worries, neither does Angelina Jolie.
Confess ... are you looking for your tape measure right now?


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The Need For Change
Over the past four years, our client had undergone several reorganizations, finally consolidating several disparate operations and acquired businesses. Significant process improvements were then implemented to adjust for changing sales volumes, intensified expense pressures and growing market competitiveness. These efforts delivered more efficient services, but the rate of change and impact were both too gradual to meet business needs. Given our client's urgent need for accelerated and dramatic improvement in terms of expense reduction, combined with distribution pressures to transition from a functional to a customer-oriented organization, the decision was made to partner with the Robert E. Nolan Company to accomplish these objectives. The immediate goals were to eliminate $2 million in expenses and transition to a client-centric service model in support of a new service strategy being implemented company-wide. The project was set to focus on the high-potential customer-facing areas and the surrounding transaction processing teams. The project followed a sequence of deliverables, each building upon the prior one:
Selection and role definition for the Core Team and Steering Committee.
Establish goals to achieve the $2 million target reduction in expenses.
Identification, quantification, and mapping of key services and transactions, creating a common foundation of knowledge for group members.
Redesign of processes and transactions, striving for innovative, out-of-the-box ideas that would accomplish the stated objectives.
Organization, consolidation, and evaluation of the redesign and improvement ideas, resulting in a list of quantifiable, actionable, and achievable recommendations.
Creation of an implementation plan outlining the steps necessary to accomplish each recommendation, noting responsible parties and measurable milestones.The workshop process was scheduled for completion in a 12-week timeframe, with the 13-member team jointly presenting the finalized implementation plan. With the Core Team containing representatives from all of the potentially affected areas, organizational buy-in to the recommendations was assured.
Summary Findings
The process improvement ideas generated during the workshop redesign sessions showed a number of commonalities:Transactional specialization, backlogs, and limited training were creating handoffs, delays, duplication of effort, and even a few extraneous units—all adding to the expense structure and detracting from service quality.
Misalignment of staff and processes, in part the result of incremental and segmented organizational growth, was causing inefficiencies and clouding ownership—in effect, erasing individual account-ability for completing a service transaction in totality.
Focus on benign call center, without counter-balancing focus on off-phone transactions (often found to be the source of the calls) was resulting in "over servicing" of the phones and failure in completing customer service requests.
Resource mis-utilization (a direct result of being limited to single job grades for entire functions with minimal service request segregation) was resulting in higher compensated staff servicing the simplest to the most complex requests indiscriminately.
Surplus staff serving limited or archaic purposes within the context of the current organization and its needs (likely from changes in direction and prior rapid reorganizations, found throughout the organization) was perpetuating inefficiencies associated with validating the roles played.
After 12 weeks, the Core Team brought its sponsor and the Steering Committee a series of implementation plans supporting 14 distinct recommendations. These recommendations were set to knock $2.2 million in annualized savings off a $10 million budget in less than one year. Key aspects of the 14 recommendations included:
Eliminating specialized, handoff-oriented units by placing responsibility for completing a transaction with the original person receiving the request.
Adjusting service standards, coverage hours and off-phone time management to reflect a combination of optimized resource utilization and customer service expectations.
Consolidating similar transaction processing units so that all like transactions are processed in the same area, under a common once-and-done framework.
Implementing a transaction and call tier structure that aligned simpler calls and requests with lower-cost resources while focusing experienced staff on more complex requests.
Restructuring the training process and supporting curriculum to expeditiously put new staff in productive, but limited roles, then following up with recurring and subject-matter-specific training modules.
Redefining managers' jobs to focus on staff development, service monitoring, quality checking, and problem resolution while removing and centralizing some non-core, administrative activities.
The team also produced 12 ancillary recommendations that involved other areas or focused on unmeasured organizational improvements. While no financial value was associated with these recommendations, an additional $1 million or so to the bottom line over time is estimated.
In the four-month project, the Core Team successfully defined a set of recommendations that would generate over $2.2 million in expense savings over the next six to nine months. An organizational structure that focused on first-call resolution and once-and-done processing was developed to position the service area for growth, while ensuring efficient and effective customer service. Job tiers and career paths were outlined that benefited employees by providing growth opportunities associated with rewards, while better matching the cost of resources with the complexity of the transaction.
One of the senior leaders of the steering committee asked the team if the process they had undergone was one they had learned from and would be able to duplicate on their own in the future. Every member of the Core Team answered in the affirmative, many vigorously. The combination of meaningful change, measurable benefits, and knowledge transfer came together to deliver bottom-line results.
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Ражњићи су популарни специјалитет са роштиља на ражњу, еквивалент грчком сувлакију, бугарском шишчета и турском шашлику. Име је изведено из речи ражањ. Јело је популарно у кухињи земаља Балканског полуострва.

Референце

Српска кухиња
Бугарска кухиња
Балканска кухиња


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Arsenal News Arsenal previews
Portsmouth believes the fans at 'Fortress' Fratton Park can help upset Arsenal
By Admin Pat - 2 March 2020, 11:55
Just because Arsenal are FA Cup specialists and Portsmouth are currently down in League One, everyone thinks that today's game should be just a formality for the Gunners, but right now there are other factors to be taken into consideration.
Firstly, Arsenal's away form has been extremely woeful in this campaign with just 3 wins in our last 15 games on the road, while at Fortress Fratton Park, Portsmouth's only home defeat this season was in a League Cup game back in September. The Pompey captain Tom Naylor thinks that the home fans could make a big difference in this cup tie. He told the Portsmouth FC website: "It's going to be tough – there's no doubt about that – and we just have to make sure we give it our all on the night.
"Our ground is a fortress and the atmosphere is crazy. I'm sure it's something that our opponents will have to adapt to.
"Who knows what can happen – our form at Fratton Park is brilliant – but we just have to enjoy the occasion.
"I watched Arsenal the other night and the front four were absolutely frightening, while they have a lot of experience.
"You don't know what sort of side they're going to put out, but even their back-up players are internationals.
"We take every game as it comes and the league is our priority, while these cup ties are an added bonus.
"We're into the fifth round to play Arsenal and we're also going to Wembley for a final – just as we did last season.
"It's massive for this club and it would be fantastic if we could get through to the quarter-finals of the FA Cup."
I must admit that until today I didn't consider Portsmouth as much of a threat, but when you look at the bare bones of the form, they could have a possible giant-killing in them. Let's hope they go easy on us!
I remember the Pompey Chimes ringing out over the years.
The old uns on here will know what I mean
Proper fans down there as well GB.Their away support is massive for a 3rd Tier club
Yes Phil they have always had terrific support, home and away.
lcebox says:
Once the pitch is decent and our players dont think they just have to turn up we should win.
I was saying on another post we shall see how Arteta's team management skills are by the way we respond to last week.
I'm sure we will turn up and with some players coming in for mins. I think we should win 3-1.


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We cultivate an ongoing conversation across the nation with organizers of local technical events who have technical backgrounds. By organizing, we are able to help industry leaders find, educate, and create awareness with our reputable technical audience. We also help our technically skilled organizers to establish a new rapport with industry leaders. Are you already an organizer? Use the Organizers Guide for more help. We provide learned best practices from our current organizers on getting started, the effort involved, building audiences, and how you can benefit.