text:
\section{Introduction}

White dwarfs (WDs) represent the final evolutionary stage for over
90\% of all stars (initial mass ${\rm M}_i < 8 \, {\rm
M}_{\small{\odot}}$). Due to very high mass loss at the tip of the
Asymptotic Giant Branch (AGB), WD progenitors lose part of their
envelope, forming a planetary nebula in their subsequent evolution. The
remaining core of the star rapidly evolves toward high effective
temperatures (\mbox{$\mbox{$T_{\rm eff}$} > 100\,000$~K}). When \element{H}- and
\element{He}-shell burning cease, the star enters the WD cooling
sequence. The evolution of these post-AGB objects is separated into a
H-rich and H-deficient sequence with a ratio of about 4:1.

In their catalog of spectroscopically confirmed white dwarfs from the
Sloan Digital Sky Survey \citep[SDSS,][]{2000AJ....120.1579Y} Data
Release 4 \citep[DR4,][]{sdss...dr4}, \citet{2006wdc...dr4E} report
31 DO white dwarfs and 10 PG~1159 stars. Following our spectral
analyses of 16 hot \element{H}-deficient objects from the DR4 WD catalog
\citep[10 DOs, of which 9 were classified as DOs and one as DB+M, 5 PG~1159
stars, and one sdO;][]{2005A&A...442..309H} which were included in DR3
\citep{2005AJ....129.1755A}, we now extend this work to 13 DOs and 4
PG~1159 stars which are available only since DR4. The
{remaining} 9 DOs from the DR4 WD
catalog not analysed in this or our previous paper are either too
noisy or insufficiently flux calibrated for a reasonable spectral
analysis.

\subsection{PG~1159 stars}

PG~1159 stars are evolutionary transition objects between the hottest
post-AGB and WD phases. The prototype of this spectroscopic class,
PG~1159-035, was found in the Palomar Green (PG) survey
\citep{1986ApJS...61..305G}. It shows a spectrum without detectable
H-absorption lines. It is dominated by \ion{He}{ii} and highly ionised
carbon and oxygen lines. PG~1159 stars are characterised by a broad
absorption trough around 4670~\mbox{${\rm \AA}$~} composed {of} \ion{He}{ii}
4686~\mbox{${\rm \AA}$~} and several \ion{C}{iv} lines, suggesting high effective
temperatures. Spectral analyses {yield} $\mbox{$T_{\rm eff}$} = 75\,000 -
200\,000$~K and gravities of $\mbox{$\log\,g$} = 5.5 - 8.0$
\citep{1991A&A...244..437W,1994A&A...286..463D,1996aeu..conf..229W}.
{Of the 28 PG~1159 stars known prior to the SDSS, ten are
low-gravity \citep[subtype lgE, ][]{1992LNP...401..273W} stars,
placing them in the same Hertzsprung-Russell-Diagram (HRD) region as
the hot central stars of planetary nebulae (CSPNe), while the others
are more compact objects with surface gravities of WDs (subtype A or
E).} Due to their {rarity}, the majority of the known
PG~1159 stars were discovered in large surveys \citep[Palomar Green,
Hamburg Schmidt (HS), ][]{1995A&AS..111..195H}. The most
recent and only discovery within the last 10 years, besides those from
the SDSS \citep{2004A&A...424..657W}, was an object from the Hamburg
ESO (HE) survey \citep{1996A&AS..115..227W}. The SDSS thus offers a
new and relatively unique opportunity to increase the number of known
PG~1159 stars.

The star PG~1159-035 (= GW Vir) also defines a class of variable
stars. \citet{1979wdvd.coll..377M} discovered low-amplitude non-radial
$g$-mode pulsations in this object. About one third of the PG~1159 stars show this
variability which is thought to be driven by cyclic ionisation of
carbon and oxygen as suggested by \citet{1986HiA.....7..229C} and
\citet{1987fbs..conf..309S}. {Analyses of HST spectra of
spectroscopically identified PG~1159 stars indicate that there is a
likely relation between high carbon and oxygen abundances and pulsations}
\citep[][hereafter DH98]{1998A&A...334..618D}, which is corroborated
by theoretical calculations of \citet{2004ApJ...610..436Q}.

The region in the HRD occupied by the PG~1159 stars overlaps
with that of the DO white dwarfs. Therefore, it is assumed that
gravitational settling of the heavier elements in the atmosphere of
the PG~1159 stars leads them to transition towards DO white dwarfs.

\subsection{DO white dwarfs}

White dwarfs can be separated into two distinct spectroscopic classes,
DA and non-DA white dwarfs. The former show a pure hydrogen spectrum
and can be found over the entire WD cooling sequence. The latter fall
into three subclasses: DO (\mbox{$45\,000~{\rm K} < \mbox{$T_{\rm eff}$} <
120\,000$~K}), DB (\mbox{$11\,000~{\rm K} < \mbox{$T_{\rm eff}$} < 30\,000$~K}), and
DC / DQ / DZ white dwarfs (\mbox{$\mbox{$T_{\rm eff}$} < 11\,000$~K}; pure continuum
/ carbon / metal lines present). The spectroscopic appearance of the
DO and DB subclasses is determined by the ionisation balance of
\ion{He}{i} and \ion{He}{ii}. DO white dwarfs show a pure \ion{He}{ii}
spectrum at the hot end and a mixed \ion{He}{i/ii} spectrum at the
cool end. The transition to the cooler DB dwarfs, characterised by
pure \ion{He}{i} spectra, is interrupted by the so-called \mbox{``DB
gap''} \citep{1986ApJ...309..241L}. In the HRD region of white dwarfs
with \mbox{$30\,000~{\rm K} < \mbox{$T_{\rm eff}$} < 45\,000$~K}, no objects with
H-deficient atmospheres have been observed to date. However,
\citet{2006dbgapE} describe over 25 objects taken from DR4 data which
likely fall in that temperature region. These new objects might
increase our knowledge of the spectral evolution of \element{He}-rich
white dwarfs considerably.

Additional constraints on stellar parameters may result from the
analysis of DO white dwarfs in binary systems. Currently, three DOs
with late type companions (PG~0046+078, PG~0237+116, and HD~149499~B)
are known. The first two have M-star companions with only a minor
contribution to the combined spectrum
\citep{1996A&A...311L..17H,1985ApjS...58..379W}. The latter one is
accompanied by a much brighter K-star which complicates the analysis of the
optical spectrum of the DO \citep{1979MNRAS.187...17W}.

As in the case of PG~1159 stars, the most recent discovery of a DO
white dwarf comes from the HE survey \citep{2004A&A...424..657W}, while
the PG and HS surveys have contributed the majority of the 19 DOs known
prior to the SDSS.

\section{Spectral Analysis}
\label{sec:specan}

In order to analyse the DO and PG~1159 spectra \citep[SDSS
  observations for these objects are described
  in][]{2005A&A...442..309H}, we calculated homogeneous,
  plane-parallel, non-LTE model atmospheres with a code based on the
  Accelerated Lambda Iteration method \citep[][ and
  references therein]{2003ASPC..288...31W}. For these types of stars,
  it is necessary to account for non-LTE effects in our
  models, as shown by \citet{1996A&A...314..217D} for DO white dwarfs
  and by \citet{1991A&A...244..437W} for PG~1159 stars. To compare
  our synthetic spectra to the observed spectra, we normalise the
  observed spectra with third order polynomials fit through the
  continua. The continua are determined by the normalised theoretical spectra.
  Lineshifts due to radial velocities are taken into account
  by means of cross-correlation.  This comparison procedure is
  performed by an \texttt{IDL} code routine in order to guarantee
  consistent results. We used a $\chi^2$-statistic to derive best-fit
  models and computed 1-$\sigma$ errors following \citet{1986ApJ...305..740Z}.

\subsection{Spectral analysis of PG~1159 stars}

For the PG~1159 stars {in our sample}, we calculated model atmospheres
using detailed
\element{H}\,--\,\element{He}\,--\,\element{C}\,--\,\element{N}\,--\,\element{O}
model atoms. The model grid ranges from \mbox{$\mbox{$T_{\rm eff}$}= 55\,000 -
150\,000$~K} and \mbox{$\mbox{$\log\,g$} = 5.5 - 7.8$}. The abundances are fixed to
values $\element{He}/\element{H}=100$ and
$\element{C}/\element{He}=0.01$, $0.03$, $0.05$, $0.07$, $0.09$,
$0.10$, $0.11$, $0.20$, $0.30$, or $0.60$ by number. We have a nearly
complete model grid with $\mbox{$T_{\rm eff}$}=55\,000 - 110\,000$~K in steps of
$5\,000$~K, $\mbox{$\log\,g$}=6.4 - 7.8$ in steps of $0.2$~dex, and
$\element{C}/\element{He}=0.01-0.11$ in steps of $0.02$. Complete
coverage of the whole parameter space is not yet available due to the
high computational time required to compute the model
atmospheres. However, the majority of the analysed PG~1159 stars are
covered by our nearly complete model grid. Best-fit models for PG~1159
star candidates were calculated with an oxygen abundance following the
typical PG~1159 abundance-scaling ratio $\element{O}/\element{C}
\approx \element{C}/\element{He}$. However, variations in the oxygen
abundance do not {produce} a significant effect on the other stellar
parameters. The nitrogen abundance is kept fixed at
$\element{N}/\element{He}=0.01$ by number which is a typical upper
limit for PG~1159 stars. Analysed spectra of PG~1159 stars together
with their best-fit models are shown in Fig.~\ref{fig:pgcomp}.

\subsection{Spectral analysis of DO white dwarfs}
\label{sec:specan_do}

Detailed \element{H}\,--\,\element{He} atomic models
\citep{1996A&A...314..217D} were used to calculate our model
atmospheres. The model grid ranges from
\mbox{$\mbox{$T_{\rm eff}$} = 40\,000 - 120\,000$~K} in steps of $2\,500$~K,
\mbox{$\log\,g$}\, ranges from 7.0 to 8.4 in intervals of 0.2 dex. The helium abundance
\begin{figure*}[ht!]
  \centering
  \includegraphics[bb= 77 365 608 774,clip,width=18cm]{4869fig1.ps}
  \caption{Normalised optical spectra (grey lines) of PG~1159 stars
    and the sdO star (bottom spectrum) along with model atmosphere fits (black
    lines). The top object shows ultra-high excitation ion
    features. Object names are printed on the left, with effective
    temperatures, logarithmic surface gravities, and carbon abundances
    (\element{C}/\element{He}), on the right.}
  \label{fig:pgcomp}
\end{figure*}
is fixed to $\element{He}/\element{H}=99$. The spectra of our analysed DOs,
together with their corresponding best-fit models, are shown in
Fig.~\ref{fig:docomp}.

\begin{figure*}[ht!]
  \centering
  \includegraphics[bb= 77 365 608 774,clip,width=18cm]{4869fig2.ps}
  \caption{Normalised optical spectra (grey lines) of DO white dwarfs
  along with model atmosphere fits (black lines).  The two top objects show
  ultra-high excitation ion features. Object names are printed on the
  left, effective temperatures and logarithmic surface gravities on
  the right. The spectra of the hottest stars are dominated by
  \ion{He}{ii} absorption lines, while increasing line strengths of
  \ion{He}{i} are observed with decreasing temperature.}
  \label{fig:docomp}
\end{figure*}

\subsection{Analysis of spectra showing DO and M dwarf features}

In order to derive stellar parameters for both stars from the DO+M
star spectra, we used the DO model atmospheres previously described in
Section~\ref{sec:specan_do} along with theoretical LTE M-star atmospheres
calculated with the \texttt{PHOENIX} code \citep{ng-hot}. Their
construction follows the setup used for the preliminary GAIA grid
\citep{inesGAIA}, but has been updated to use \texttt{PHOENIX} version
14.1 and compute spectra at 0.2 {\AA} resolution. Major updates to the
input physics include the adaption of the revised solar composition of
\citet{2005ASPC..336...25A} for the chemical equilibrium abundances and a
correction to the partition sum for TiO, leading to $\sim$\,3-times
greater line strengths for this important absorber (Allard et al., in
prep.).

For the fit of both spectral components, a Planck spectrum was {first} fitted
to represent the Rayleigh-Jeans tail contribution of the DO in the red
part of the spectrum; then we selected a model spectrum based on an
initial fit of the spectral type of the cool companion and subtracted
it from the observation. Next, we used our $\chi^2$-fitting
routines to determine the best DO fit. This model was then subtracted
from the combined observed spectrum and the remaining cool star
spectrum was fitted to a grid of models spanning $\mbox{$T_{\rm eff}$} = 2600-5000$~K
in steps of $100$~K and $\mbox{$\log\,g$}= 3.5-5.5$ in steps of $0.5$ dex. The best
fit was determined by $\chi^2$-minimisation over the entire spectral
range; however we assigned a reduced weight to the regions from
6430\,--\,6560 \AA\ and 6720\,--\,6950\,{\AA}. In this part of the TiO
bands, the models reproduce the observations rather poorly, as has been
noted in previous analyses of M dwarfs
\citep[e.\,g.][]{MLTbinaries}. A reason for this mismatch is probably
superposed absorption due to CaH, for which no line opacity data are
available in the \texttt{PHOENIX} version used for these models.
Despite these shortcomings we find acceptable fits for SDSS
J091621.83+052119.2 and SDSS J133633.22$-$013116.5 at
3600\,--\,3700\,K, with the fit quality rapidly degrading towards
higher and lower {\mbox{$T_{\rm eff}$}}.  In light of the unknown systematic errors
due to the incomplete molecular data, flux calibration errors, and
possible interstellar reddening, we conservatively estimate an
uncertainty in {\mbox{$T_{\rm eff}$}} of 100\,K. The much fainter spectrum of the
companion to SDSS J075606.36+421613.0 is consistent with temperatures
from at least 3000\,--\,3600\,K.  In all cases, the spectra show very
little sensitivity to gravity within a range of $4.0 < \mbox{$\log\,g$} < 5.5$. A
direct determination of the stellar radius is therefore not possible
from these data, but the fits are entirely consistent with the
assumption of main sequence stars and the companion radius can
therefore be determined from a standard mass-radius-relation as well
as from evolutionary tracks.  We did not find any improvement of the
fits using metallicities either higher or lower than solar.

Finally, we subtracted the best-fit M-star model atmosphere from the
observed spectrum and used our standard $\chi^2$-fitting routines
again to refine \mbox{$T_{\rm eff}$}\ and \mbox{$\log\,g$}\ for the DO white dwarf.  Only minor
differences in effective temperatures and surface gravities compared
to the first DO model fit were derived. The three spectra showing DO
and M-star features together with combined DO and M-star models are
presented in Fig.~\ref{fig:dom}.

\begin{table*}[ht!]
  \caption{Photospheric parameters of our PG~1159 star sample. The
  \element{C}/\element{He} abundance ratio is given by number. Objects
  marked with an asterisk ($^\ast$) have been analysed in
  \citet{2005A&A...442..309H}. The PG~1159 stars which have
  been observed for pulsations do not show variations above the specified
  detection limit $\sigma$.}
  \label{table:1}
  \centering
  \begin{tabular}{l r @{\,$\pm$\,} l r @{\,$\pm$\,} l r @{\,$\pm$\,} l
    l}
    \hline\hline\noalign{\smallskip} Name & \multicolumn{2}{c}{\mbox{$T_{\rm eff}$}}
    & \multicolumn{2}{c}{\mbox{$\log\,g$}} &
    \multicolumn{2}{c}{\element{C}/\element{He}} & remarks\\
    SDSS J & \multicolumn{2}{c}{[kK]} & \multicolumn{2}{c}{[cgs]} &
    \multicolumn{2}{c}{} & \\
    \hline
    001651.42$-$011329.3$^\ast$ & 120.0&2.3 & 5.50&0.49  &
    0.30&0.006 & \\
    102327.41+535258.7$^\ast$   & 110.0&1.6 & 7.60&0.03  &
    0.20&0.007 & non-variable ($\sigma=12$~mmag)\\
    142555.47+531525.1      & 110.0&0.9 & 7.60&0.01 &
    0.20&0.004 & known as PG~1424+535 (DH98) \\
    075540.94+400918.0$^\ast$   & 100.0&2.6   & 7.60&0.05 &
    0.03&0.006 & \\
    093546.53+110529.0          & 100.0&1.3 & 7.60&0.03 &
    0.05&0.002 &  non-variable ($\sigma=15$~mmag)\\
    121523.09+120300.8      & 100.0&0.8 & 7.60&0.02 &
    0.05&0.002 & shows ultra-high excitation ion absorption \\
    134341.88+670154.5$^\ast$   & 100.0&0.7 & 7.60&0.02 &
    0.05&0.001 & non-variable ($\sigma=9$~mmag)\\
    144734.12+572053.1$^\ast$   & 100.0&1.6 & 7.60&0.02 &
    0.05&0.002 & non-variable ($\sigma=10$~mmag)\\
    034917.41$-$005919.3        &  90.0&0.9 & 7.50&0.01 &
    0.30&0.019 & \\
    \hline
    233541.47+000219.4     &  60.0&0.9 & 6.40&0.01 &
    0.01&0.001 & (sdO) known as WD~2333$-$002 \\
    110215.46+024034.2$^\ast$   &  55.0&0.8 & 6.40&0.02 &
    0.01&0.003 & (sdO) \\
    \hline
  \end{tabular}
\end{table*}

\section{Results and discussion}

After presenting ten DO white dwarfs and five PG~1159 stars in
\citet{2005A&A...442..309H}, we now extend our spectral analyses to
the recently published SDSS DR4 DOs and PG~1159 stars. We present
results from this work and \citet{2005A&A...442..309H} together in
Table~\ref{table:1} and Table~\ref{table:2}. Some atmospheric
parameters for the PG~1159 stars analysed in
\citet{2005A&A...442..309H} have changed after applying our
$\chi^2$-fitting routines to these objects. The statistical
errors provided by the $\chi^2$-analysis and presented in
Table~\ref{table:1} and Table~\ref{table:2} are very small, while
suspected systematic errors are of the order of the grid steps
described in Section~\ref{sec:specan}.

\subsection{PG~1159 stars}

We found six spectra from the SDSS DR4 WD catalog
\citep{2006wdc...dr4E} which we identified as PG~1159 stars, although
one (SDSS J233541.47+000219.4) turns out to be best fit as a sdO
rather than a PG~1159 star, even though strong \ion{C}{iv} lines are
present. Our model grid is not adopted for the analysis of sdO stars
and the results are therefore preliminary only. We note that the
\ion{He}{ii} line cores are not well matched with the current best-fit
model. This object, known as WD~2333$-$002, has been previously
classified by \citet{2005ApjS..156...47L} as a sdB/sdOB.

One of our six selected PG~1159 stars, SDSS J114635.23+001233.5, was
previously known as PG~1144+005. Since no new model atmospheres for
this hot object are available, the photospheric parameters
$\mbox{$T_{\rm eff}$}=150\,000$~K, $\mbox{$\log\,g$}=6.50$, and $\element{C}/\element{He}=0.50$
derived by \citet{1991A&A...247..476W} still hold and the spectrum is
not analysed in this work.

SDSS J121523.09+120300.8 shows features of ultra-high excitation ions
(uhei) and is the first PG~1159 star of that type discovered so
far. Lines of \ion{O}{vii} and \ion{N}{vii} around 3888~\AA, at
5673~\AA, and around 6086~\AA, as well as \ion{O}{viii} at 4340~\AA,
4658~\AA, and 6064/6068~\AA\ are clearly visible in the spectrum (see
Fig.~\ref{fig:pgcomp}). Absorption features of \ion{C}{vi},
\ion{N}{vi}, \ion{Ne}{ix}, and \ion{Ne}{x} described by
\citet{1995A&A...303L..53D}, \citet{1995A&A...293L..75W}, and
\citet{2004A&A...417.1093K} for DO white dwarfs, are also indicated in
Fig.~\ref{fig:pgcomp} and are only ambiguously identifiable due to
low signal-to-noise and spectral resolution. The observed \ion{He}{ii}
absorption lines are too deep to be fitted with any model. Due to the
lack of appropriate modelling of the uhei phenomenon, stellar
parameters are derived for this star from a best-fit model which is
determined without considering the uhei lines. It should be kept in
mind that significantly higher temperatures (\mbox{$T_{\rm eff}$}$\,>\,500\,000$~K)
are necessary to excite the uhei lines visible in this spectrum
\citep{1995A&A...303L..53D}.

\begin{figure*}[ht!]
  \centering \includegraphics[bb= 76 370 536
  560,clip,width=18cm]{4869fig3.ps}
  \caption{Positions of the PG~1159 stars (black diamonds) analysed in
    this paper compared to evolutionary tracks from
    \citet{1995A&A...299..755B} and \citet{1983ApJ...272..708S} (dashed
    lines), and \citet*{1986ApJ...307..659W} (solid lines). The sdO star
    from this work (black asterisk) and the one from
    \citet{2005A&A...442..309H} are plotted together with tracks from
    \citet{1993ApJ...419..596D} (dash-dotted lines). Statistical error
    bars for all analysed objects are smaller than the symbols. The plot
    also includes previously known PG\,1159 stars and proposed progenitor
    objects (early and late Wolf-Rayet CSPNe:[WCE],
    [WCL], and [WC]-PG~1159). Labels: mass in M$_{\small{\odot}}$.}
  \label{fig:trackpg}
\end{figure*}

The remaining three PG~1159 star candidates are A subtype PG~1159
stars. SDSS J142555.47+531525.1 was already known as PG~1424+535 or
WD~1424+535 and has been analysed by DH98 and
\citet{1991A&A...244..437W} who derived
$\mbox{$T_{\rm eff}$}=110\,000$~K/$100\,000$~K, respectively, $\mbox{$\log\,g$}=7.00$, and
$\element{C}/\element{He}=0.30$ using UV and optical HST spectra. Our
fit provides the same effective temperature as DH98, but a higher
surface gravity ($\mbox{$\log\,g$}=7.60$), and a lower carbon abundance
($\element{C}/\element{He}=0.20$) for the new SDSS spectrum of this
object. In our analysis we also fit the spectrum with the model used
by DH98, but we {obtained} a slightly lower $\chi^2$-value for our new
model. However, the models used are not very sensitive to carbon
abundance changes above $\element{C}/\element{He} \approx 0.10$ in the
optical.

The stellar parameters resulting from these spectral analyses are
listed in Table~\ref{table:1}. We have also included results from
time-resolved photometric observations of four candidates for pulsating
PG~1159 stars in Table~\ref{table:1}, obtained at the Calar Alto
Observatory 2.2~m telescope in March 2005. In Fig.~\ref{fig:trackpg},
positions of the four analysed PG~1159 stars and the one sdO star are
compared with evolutionary tracks as well as positions of previously
known PG~1159 stars including those from DR3
\citep{2005A&A...442..309H}.  The typical SDSS
PG~1159 star has approximately $\mbox{$T_{\rm eff}$}=100\,000$~K, $\mbox{$\log\,g$}=7.5$, and
$\element{C}/\element{He}=0.05-0.30$.

The position of SDSS J233541.47+000219.4 favours our classification of
it as a sdO star. It fits the evolutionary tracks of
\citet{1993ApJ...419..596D} within the tiny error bars very well and
therefore suggests an Extended Horizontal Branch rather than an AGB
history.

\subsection{DO white dwarfs}

Stellar parameters for 13 previously unanalysed DO white dwarfs are
presented in Table~\ref{table:2}. Three objects show M-star features
in their spectra and two display uhei lines \citep[classified
by][]{2004A&A...417.1093K}. Table~\ref{table:notana} lists the
DO white dwarfs from the DR4 WD catalog not analysed here -- mainly
because their spectra are too noisy.

The two uhei DO white dwarfs show absorption lines of \ion{O}{vii} and
\ion{N}{vii} around 3888~\AA, at 5673~\AA, and around 6086~\AA, as
well as \ion{O}{viii} at 4340~\AA, 4658~\AA, and
6064/6068~\AA. \ion{Ne}{ix} signatures are also present in SDSS
J025403.75+005854.4. The \ion{He}{ii} lines, especially the one at
6556~\AA, are very strong and cannot be fitted by our models. As
mentioned above, the effective temperature required to excite these ions to
a degree as detected in the two uhei DOs exceeds $500\,000$~K. A
massive post-AGB remnant of 1.2~\mbox{$M_{\odot}$}\ can reach effective
temperatures up to $700\,000$~K on very short time scales
\citep{1970AcA....20...47P}, yet, \citet{1995A&A...293L..75W} argue
that uhei features in DO white dwarfs cannot be of photospheric origin
since \ion{He}{ii} lines would disappear completely at such high
temperatures. The hypothesis of optically thick and hot stellar winds
was proposed by the authors due to the triangular shape of the line
profile. Furthermore, the lines are blue shifted, which favours the
\begin{figure}[ht!]
  \centering \includegraphics[bb= 81 365 462
  684,clip,width=8.8cm]{4869fig4.ps}
  \caption{Mass distribution (bin\,=\,0.1\,\mbox{$M_{\odot}$}) of all known DO
    white dwarfs. The black bars represent masses of stars from this
    work while the area under the black lines shows results from all
    the SDSS spectral analyses \citep[][ and this
    work]{2005A&A...442..309H}.}
  \label{fig:massdis}
\end{figure}
assumption of an expanding envelope. Neglecting this very hot
component in the spectral analyses, the uncertainties given by the
$\chi^2$-fitting procedure are likely to be lower than the systematic
errors due to incomplete modelling of the uhei phenomenon.
\begin{table}[ht!]
  \caption{Stellar parameters of our SDSS DO white dwarf sample. The
    three objects
    below the line show spectra with DO and M-star features. The letters
    A and B denote the DO and the M-star component, respectively. Objects
    marked with an asterisk ($^\ast$) have been previously analysed in
    \citet{2005A&A...442..309H}.}
  \label{table:2}
  \centering
  \begin{tabular}{l r @{\,$\pm$\,} l r @{\,$\pm$\,} l c}
    \hline\hline\noalign{\smallskip} Name & \multicolumn{2}{c}{\mbox{$T_{\rm eff}$}}
    & \multicolumn{2}{c}{\mbox{$\log\,g$}} & M \\
    SDSS J & \multicolumn{2}{c}{[kK]} & \multicolumn{2}{c}{[cgs]} &
    [\mbox{$M_{\odot}$}] \\
    \hline
    091433.61+581238.1$^\ast$   &120.0&1.7  & 8.00&0.02 & 0.75  \\
    204158.98+000325.4$^\ast$   &110.0&4.5    & 7.20&0.04 & 0.60  \\
    214223.32+111740.4          &110.0&2.4 & 7.60&0.05 & 0.60  \\
    154752.33+423210.9$^\ast$   & 100.0&1.6  & 7.60&0.06 & 0.59 \\
    151026.48+610656.9$^1$      & 95.0&0.8 & 8.00&0.04 & 0.71 \\
    084008.72+325114.6$^\ast$   & 85.0&1.1  & 8.40&0.08 & 0.90 \\
    025403.75+005854.4$^1$      & 80.0&0.5 & 8.00&0.06 & 0.68 \\
    155356.81+483228.6$^\ast$   & 75.0&1.2  & 8.00&0.09 & 0.68 \\
    084223.14+375900.2          & 70.0&0.3 & 8.00&0.06 & 0.68  \\
    140409.96+045739.9$^\ast$   & 70.0&0.5  & 8.00&0.04 & 0.68  \\
    113631.50+591229.8          & 67.5&1.6 & 8.20&0.13 & 0.78 \\
    131724.75+000237.4$^{\ast,2}$ &  62.5&0.5  & 7.80&0.03 & 0.58 \\
    034101.39+005353.0$^\ast$   & 55.0&0.4  & 8.00&0.05 & 0.65 \\
    003343.06+142251.5          & 52.5&0.2 & 8.20&0.01 & 0.76 \\
    115218.69$-$024915.9        & 52.5&0.3 & 8.20&0.02 & 0.76  \\
    034227.62$-$072213.2$^\ast$ & 50.0&0.2  & 8.00&0.03 & 0.65 \\
    081115.09+270621.8          & 48.0&0.3 & 8.00&0.04 & 0.64 \\
    113609.59+484318.9$^{\ast,3}$ &  48.0&0.1  & 8.00&0.04 & 0.64 \\
    081546.08+244603.3          & 48.0&0.2 & 8.20&0.01 & 0.76 \\
    015629.58+131744.7          & 40.0&0.2  & 8.20&0.01 & 0.75 \\
    \hline
    091621.83+052119.2 (A)   & 60.0&5.0 & 8.00&0.20 & 0.66 \\
    091621.83+052119.2 (B)   &  3.7&0.1 & 4.75&0.50 & 0.51 \\
    133633.22$-$013116.5\ A  & 52.5&0.5 & 7.60&0.06 & 0.48 \\
    133633.22$-$013116.5\ B  &  3.6&0.1 & 4.75&0.50 & 0.45 \\
    075606.36+421613.0\ A    & 52.5&0.8 & 7.40&0.05 & 0.42 \\
    075606.36+421613.0\ B    &  3.2&0.2 & 5.00&0.50 & 0.18 \\
    \hline
    \multicolumn{6}{l}{$^1$ shows ultra-high excitation ion absorption}\\
    \multicolumn{6}{l}{$^2$ previously known as HE~1314+0018
    \citep{2004A&A...424..657W}}\\
    \multicolumn{6}{l}{$^3$ previously known as WD~1133+489
    \citep{1997fbs..conf..303D}}\\
  \end{tabular}
\end{table}

SDSS J003343.06+142251.5 and SDSS J015629.58+131744.7 have been
classified by \citet{2004A&A...417.1093K} as DBAO and DBO,
respectively, while the former is listed as DO and the latter as DBO
in the DR4 WD catalog. Comparing the spectrum of the former object to
our DO models, we note that \ion{He}{ii} lines at 4686~\AA, 5412~\AA,
and 6563~\AA\ are stronger in the model than in the
observation. \ion{He}{i} is well fitted in the whole spectrum. In
contrast, \ion{He}{i} lines at 4026~\AA\ and 4471~\AA\ are stronger in
the observation than in the model for the latter. The
extension of the model grid to even lower model temperatures does not
improve the fit of the \ion{He}{i} lines since they are almost
saturated. The rest of the \ion{He}{i} lines in the model and the
observation match. SDSS J015629.58+131744.7 appears to be the coolest
DO known to date. The addition of small amounts of hydrogen did not lead
to a better fit for SDSS J003343.06+142251.5, so that we cannot explain
the weak \ion{He}{ii} lines by traces of hydrogen in the atmosphere.

\begin{figure*}[ht!]
  \centering
  \includegraphics[bb= 74 372 534 560,clip,width=18cm]{4869fig5.ps}
  \caption{Positions of DO white dwarfs compared with evolutionary
  tracks from \citet{1995LNP...443...41W}. The triangles represent the
  27 hitherto known DOs
  \citep[see][]{1996A&A...314..217D,1997fbs..conf..303D,2004A&A...424..657W,2005A&A...442..309H}.}
  \label{fig:trackdo}
\end{figure*}

\begin{table}[ht!]
  \caption{DO white dwarfs from the DR4 WD catalog not analysed in
  this work due to noisy spectra or as denoted.}
  \label{table:notana}
  \centering
  \begin{tabular}{l l l}
    \hline \hline
    Name & Name \\
    SDSS J & SDSS J\\
    \hline
    011346.78+002828.7$^{1,2}$ & 140615.80+562725.9 \\
    074538.17+312205.3         & 150053.99+025143.2 \\
    081533.08+264646.4         & 205930.25$-$052848.9$^{3}$ \\
    083504.76+090111.7         & 213932.48+112611.2 \\
    130248.99$-$013309.5 & \\
    \hline
    \multicolumn{2}{l}{$^1$ insufficiently flux calibrated}\\
    \multicolumn{2}{l}{$^2$ previously known as HS~0111+0012 \citep{1996A&A...314..217D}}\\
    \multicolumn{2}{l}{$^3$ dent in spectrum at $\sim 5800$ \AA}\\
  \end{tabular}
\end{table}

Masses for all objects are derived from our photospheric parameters
and evolutionary tracks from \citet{1995LNP...443...41W}. The thirteen
analysed DOs are plotted with these tracks in Fig.~\ref{fig:trackdo} and
the mass distribution for all DO stars is shown in
Fig.~\ref{fig:massdis}. As already mentioned in
\citet{2005A&A...442..309H}, DOs from the SDSS seem to have higher
masses than those analysed before the SDSS. We assume that this is
an effect introduced by the application of our automated fitting
routines which favour good line wing fits, thus steering the fits
towards higher surface gravities.

\subsection{Combined DO and M dwarf spectra}

The three observed spectra that show both DO and M-star features, along
with combined DO and M-star model atmospheres are shown in
Fig.~\ref{fig:dom}. The flux of each model is multiplied by the
squared radius of the individual component. The radii are derived
from the surface gravity and mass which come from evolutionary tracks
from \citet{1995LNP...443...41W} for the DOs and
\citet{1998A&A...337..403b} for the M-stars. A constant factor which
accounts for our distance from the source is multiplied to DO and
M-star model fluxes. The total flux clearly fits SDSS
J133633.22$-$013116.5 and SDSS J075606.36+421613.0 within the
uncertainties, suggesting that the spectra come from binary
systems. SDSS J091621.83+052119.2, however, shows a deviation between
combined models and observation which cannot be explained by the
uncertainties {in} the stellar parameters. We therefore propose that
the spectrum originates from two {unrelated} stars on the same line of
sight. This is also corroborated by the {images of the objects, which
have ellipsoidal shapes and different photometric centres in different
colors}.\footnote{see
\url{http://cas.sdss.org/dr4/en/tools/explore/obj.asp?id=587732578300657729}}
A sum of DO and M-star models scaled \textit{individually} for distances fit
\begin{figure*}[ht!]
   \centering \includegraphics[bb= 68 365 467
  718,clip,width=18cm]{4869fig6.ps}
  \caption{Observed spectra of two DO+M binaries (bottom two grey lines)
  and of one DO white dwarf and M-star pair which are coincidentally in the same
  line of sight. Combined model atmospheres for the two components are
  shown as black lines. The black dashed line plotted over SDSS
  J091621.83+052119.1 is the combination of the DO and M-star models
  where scaling is performed for different distances.}
  \label{fig:dom}
\end{figure*}
the observation well (dashed line in Fig.~\ref{fig:dom}) showing that
the model parameters were derived properly.

Stellar parameters for the M-star components are shown
in Table~\ref{table:2}. Our fitting routines found a best-fit model
with \mbox{$T_{\rm eff}$}\,=55\,000~K for the DO part of SDSS J091621.83+052119.2
using the normalised spectrum. However, the flux distribution of the
observed spectrum favours an effective temperature of
\mbox{$T_{\rm eff}$}\,=60\,000~K. We chose the latter value since M-star contributions
in the normalised spectrum (observation minus M-star model) were still
significant. Error estimates are 0.2 dex for \mbox{$\log\,g$}\ and 5\,000~K in
\mbox{$T_{\rm eff}$}\ because the continuum distribution is not properly fitted
with parameters which exceed the range given by these errors.

\section{Summary}

We have performed spectral analyses {of} 18 hot H-deficient (pre-)
white dwarfs that are new in Data Release 4 of the Sloan Digital Sky
Survey using our $\chi^2$-fitting routines. We confirm three PG~1159
stars, one of which shows lines of ultra-high excitation ions (uhei). A
re-analysis of PG~1424+535 with our $\chi^2$-programs using a SDSS
spectrum has provided a lower carbon abundance and a higher surface
gravity than found by \citet{1998A&A...334..618D}. Furthermore,
thirteen DO white dwarfs have been analysed, two of which show uhei
absorption and three of which have M-star features in their spectra. We
propose that two of the three latter objects are binary systems.  The
mass distribution of the DO white dwarfs from the SDSS is shifted towards
higher masses compared to the one constructed from analyses before the
SDSS.

\section{Acknowledgments}

We thank Daniel J. Eisenstein for helpful discussions and comments on
the DR4 WD catalog.

We would also like to thank F. Allard for instructive comments on molecular
opacities and helpful discussions. Model atmospheres used for this work
were calculated in part on the IBM pSeries of the Gesellschaft f\"ur
wissenschaftliche Datenverarbeitung mbH G\"ottingen (GWDG).

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

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

Photometric data for the search for pulsations in PG~1159 stars are
based on observations collected at the Centro Astron\'omico Hispano
Alem\'an (CAHA) at Calar Alto, operated jointly by the Max-Planck
Institut f\"ur Astronomie and the Instituto de Astrof\'isica de
Andaluc\'ia (CSIC).

\bibliographystyle{bibtex/aa}

redpajama_set_name: RedPajamaArXiv


text:
Stamford's McDonald poised to become first openly gay chief justice
Bill Cummings, Neil Vigdor
Jan. 8, 2018 Updated: Jan. 10, 2018 4:59 p.m.
Justice Andrew J. McDonald
John Marinelli / contributed photoShow MoreShow Less
2of11Andrew J. McDonald, right, with husband, Charles Gray, left, of Stamford.Keelin Daly/STShow MoreShow Less
4of11Associate Supreme Court Justice Andrew J. McDonald, led questioning Tuesday on a Milford free-speech case.Dru Nadler / Dru NadlerShow MoreShow Less
5of11Andrew J. McDonaldKathleen O'RourkeShow MoreShow Less
7of11Andrew J. McDonald.Ben Holbrook Contributed Photo/STShow MoreShow Less
8of11Connecticut Supreme Court Justice Andrew McDonald speaks during the Stamford Coalition for Respectss Coming Out to Open Arms! event at the UConn Stamford Campus in 2014.Hearst Connecticut Media fileShow MoreShow Less
10of11McDonaldContributed Photo / John MarinelliShow MoreShow Less
HARTFORD — First, he flew the rainbow flag over the Governor's Residence.
Then Connecticut's Dannel P. Malloy clashed with his Indiana and North Carolina gubernatorial counterparts, one of them being Mike Pence, over their states' religious freedom and bathroom laws.
Now, the Malloy doctrine on LGBT rights has another cornerstone — appointing the nation's first openly gay chief state Supreme Court chief justice, Andrew J. McDonald.
The governor revealed plans Monday to nominate his longtime Stamford ally and friend to succeed retiring Chief Justice Chase T. Rogers on the seven-member court. The choice of McDonald, a former state senator and one-time general counsel to the governor, is subject to legislative approval.
McDonald, 51, has been an associate justice since 2013, the second of seven state Supreme Court picks of Malloy. Five of the current seven justices are Malloy appointees, a number that could grow to six if McDonald is confirmed.
The historical significance of his rise in the judicial branch was not lost on McDonald, who resides in Stamford with his husband, Charles Gray.
"When I was born here in Connecticut, a little more than 50 years ago, loving relationships like the one Charles and I cherish were criminal in 49 states, including Connecticut," McDonald said. "And when I came out in the early 1990s, I had family members who loved me counsel me against pursuing either a career in law or public service because of deeply ingrained prejudices held by some people. But now, because of changes brought about by the evolving understanding of people, new statutes passed by legislators and important court cases - indeed, by the rule of law - this day was made possible."
The governor characterized McDonald, a former corporation counsel for the city of Stamford when Malloy was mayor, as a revered jurist.
"He has a deep understanding of the role and the impact that the justice system has on the everyday lives of Connecticut residents, and the value of ensuring equality and fairness through the court's many responsibilities," Malloy said.
The emergence of McDonald as the new face of the scales of justice in the state was not without controversy, however.
Republican gubernatorial candidate Tim Herbst, the former Trumbull first selectman, criticized the pick as political and said that McDonald has tried to legislate from the bench. When Malloy was sworn-in to a second term as governor in 2015, it was McDonald who administered the oath of office.
"The interpretation of our laws should always remain blind to the influence of politics or even the appearance of influence and that is why I am calling on legislators, of both parties, to support a different nominee for chief justice," Herbst said. "Justice McDonald's record demonstrates a propensity for taking positions that have been deemed to be unconstitutional, and in some instances, positions that have been influenced by personal and political opinions that are in contravention to the law."
Herbst said McDonald sided with the majority when the state Supreme Court ruled Connecticut's death penalty law unconstitutional in 2015 by a 4 to 3 vote. The law had repealed capital punishment for those convicted of the most violent crimes after its passage in 2012, but did not apply to those already on death row.
The court's majority ruled that there could not be two levels of justice.
"McDonald was the deciding justice in State vs. Santiago, which disregarded the intent of the legislature and the people of Connecticut by allowing the perpetrators of the gruesome Cheshire home invasion to escape the death penalty," Herbst said.
No timetable has been set for McDonald's confirmation hearing before the Legislature's Judiciary Committee, a panel he once headed as a member of the General Assembly. The committee's co-chairman is fellow Stamford Democrat William Tong, who is exploring a run for state attorney general.
"I see it as a landmark moment for our state for equality and civil rights," Tong said of the choice of McDonald. "This nomination has nothing to do with one person. It has to do with breaking down an unjust barrier that has been there for a long time, and it's a proud moment for our state."
When McDonald was appointed by Malloy to the bench, there were just seven LGBT justices in the nation. The one-time Stamford Board of Finance chairman appears to have support on the other side of the aisle.
"Andrew McDonald will be a fair, balanced and transparent chief justice," said Republican state Rep. Livvy Floren, who represents parts of Stamford and Greenwich. "I have known Andrew as a colleague in Stamford and in the General Assembly and as a friend. He is a consummate professional with impeccable credentials - as a lawyer, legislator, and jurist. This is a great day for Andrew and for the people of Connecticut."
http://twitter.com/gettinviggy; nvigdor@hearstmediact.com; 203-625-4436
Bill Cummings
Reach Bill on
Bill Cummings is a veteran newspaper reporter who first joined the Connecticut Post in 1989 as a town reporter. He has served as a bureau chief, manned the Capitol Bureau, covered Bridgeport City Hall and was later named group Investigative Reporter. Bill also covers environmental issues for Hearst. He previously worked for the Watertown Daily Times in New York State and the Star Herald, a weekly in northern Maine.
Neil Vigdor

redpajama_set_name: RedPajamaCommonCrawl


Just imagine, Scottish company Johnstons of Elgin producing cashmere products there are more than 200 years! They, by the way, were the first in Europe who started raising a special mountain goats, and then weave hair of such pleasant to touch the fabric. From this fabric firm for many years makes excellent furniture, as, for convenience, and form. Today we want to share inspiring pictures of the latest interior design company directory. Cell beautiful!


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We all have seen these past years a photo of this awesome home. Vogue Living has made a complete house tour of it for our great pleasure. take a tour, soooo inspiring.
A restored factory in a small Umbrian town in Italy maintains its grand scale while providing the intimate comforts of home.
The imposing and characterful building that Andrea Falkner Campi calls home has seen service as a silkworm factory and a tobacco-drying tower.
Article suivant FOSTER HUNTINGTON, A MODERN HERO.


text:
Gatsby Athens Hotel, Award-Winning Architecture with Renowned Interior Design
Posted in Projects on 24 August, 2022
Gatsby Athens Hotel brings a new lease of life and avant-garde design to a previous derelict building in the historical centre of Athens. Generating a renewed energy to the Greek capital, the 33-room contemporary boutique hotel balances sophisticated design and personalised, attentive service with exciting food, beverage and entertainment offerings reflecting the best of its location's cultural and social milieu.
With interiors designed by acclaimed London and New York based design firm Michaelis Boyd, the hotel's public spaces feature unique entertaining and social spaces to suit every mood – and offer an array of dining possibilities. The architectural design was led by award-winning Greek architectural firm WOA, which has transformed the crumbling 1930's building and police station into an elegant and eco-friendly hotel rooted in the emotional connection between people and buildings. Costas Gagos Architecture and Design Studio has also recently completed the basement to curate an allusion of hidden rooms and secret passageways.
Opened in Autumn 2021, Gatsby Athens has become Athens' premium gathering place, the all-day restaurant is the main social hub of the hotel, and the rooftop garden offers a casual-cool vibe, welcoming hotel residents and guests to dine with stunning panoramic views and a glimpse of the Acropolis.
Architectural Inspiration
WOA's architectural vision balances between the typical Greek modern architectural typology, the contemporary vision of sustainable buildings, creating a meaningful experience for guests. The art deco building has been abandoned for the past four decades, so it was important to convey a sense of timelessness rather than a decade-defining aesthetic. The setting evokes the glamour of mid-1930 Athens, creating a fine balance between old and new. Simple and clean lines have been honoured throughout the design, whilst preserving as much of the original structure as possible but bringing an eco-twist with a natural green façade to the building. To honour its past and future, design intricacies have been employed that complement the building's heritage and surroundings – materials have been reused and the majority of the construction of the hotel was handmade or custom made by local craftsmen.
Here, every aspect of an urban hotel has been re-imagined for the needs and desires of a new generation, and every thought given to enhancing a guest's stay, for the best possible Athenian experience.
Gatsby Athens Hotel architecture vision balances between the typical Greek modern architectural typology, the contemporary vision of sustainable buildings and the new luxury concept of creating a meaningful experience. Simple, elegant and eco-friendly architecture rooted in the emotional connection between people and buildings with a fundamental urge of creating something truly unique", comments Aris Giannopoulos, Architect Engineer for WOA.
Inspiration Behind The Interior Design
Michaelis Boyd has made their name by creating spaces that are emotive, meaningful and thoughtful, taking inspiration from nature and considering light, form and flow.
At the heart of every space is authenticity and the design team have been careful to maintain original elements of the interior architecture whilst bringing the interiors up to date. The result is a contemporary scheme that draws on art deco influences in keeping with the Gatsby legacy. Period details such as the existing white marble staircase were preserved, and materials such as warm woods and veined marbles introduced, chosen for their timeless quality and to patinate over time. Inspired by the natural environment and the local culture and craftspeople, tactility is a key part of the design process. Layered textures are combined with contemporary furniture, touches of reeded glass and gold details for a luxurious finish that compliments traditional Greek design elements, such as the red and green marble, and locally sourced terrazzo.
We are really excited to be working with the Gatsby Athens, as it is our first boutique hotel project in Greece. At Michaelis Boyd, we believe that interior design doesn't have to conform to a rigid set of rules – we like to challenge the norm and gently encourage our clients to explore playful and intriguing elements. The Gatsby Athens was a perfect fit, as we were able to explore lots of creative options – a subtle mix of old and new, we've worked to reinstate the building's authenticity but also bring it up to date. The resulting interiors reflect the urban, subversive and underground neighbourhood vibe but remain luxurious, exclusive and elegant, to emulate the hotel's refined yet playful character." – Alex Michaelis, partner at Michaelis Boyd.
Sustainably Designed
The creation of the Gatsby Athens Hotel brought back to life a dilapidated Athenian building which was an eyesore and destined to be demolished. Reusing buildings and avoiding the CO2 emissions from construction is the most sustainable way to build. In addition, the building has been optimized for energy efficiency with the use of new technology and with the addition of high quality thermo-proofing throughout the structural elements of the building. There has also been an addition of a beautiful natural green façade to the exterior of the building.
Gatsby Athens Hotel is a contemporary boutique hotel with 33 luxurious rooms. All rooms provide state of the art technology, smart TVs or tablets, Alexa devices, king size beds, walk-in showers, in-room bathtubs, luxury natural linen and bathrobes, Ortigia amenities, impressive artwork and even a 'surprise' button for those who dare to press. All the furniture is bespoke, including most of the lighting fixtures which were designed by the Michaelis Boyd team and locally produced. Upgraded rooms come with Juliet balconies or terraces with private outdoor sitting areas, an outdoor cinema and jacuzzi hot tubs.
By understanding that a hotel is more than just a place to sleep—it's a hub, a meeting place, a centre culture, a site for relaxation, reflation, and hard-earned leisure time, and place for life and play— there is Gatsby Party Suite, for the more socially inclined who like late night revelry.
Michaelis Boyd designed the impressive bar as a sculptural statement, with an arched back bar shelving, brass and glass detailing and a marble top bar that is gently scalloped and surrounded by velvet and leather stools. On the rooftop lies a secret garden, set on the 6th floor, including an open-air cinema, a roof garden, a seasonal bar and a small viewing platform with great urban views and a glimpse of the Acropolis.
The basement has been newly refurbished and cleverly reconfigured by Costas Gagos Architecture and Design Studio to create a four zone multi-functional space. The renowned and talented team are constantly pushing limits with their designs, winning the coveted 'Designer of the Year' award multiple times. There is a discreet 24-hour detox GYM with the latest fitness equipment and a serene cave inspired massage room awaits for guests to escape and indulge in a luxurious treatment next door.
Similarly, an exclusive and cozy lounge area is canopied by a beautiful bespoke scalloped ceiling, with a sumptuous velvet couch and comfy armchairs providing the perfect space to relax. The intrigue continues with a secret door that leads the way to a speakeasy jazz bar. This basement is made to be discovered, not ignored!
Architecture and Local Surroundings
Gatsby Athens Hotel dates back to the war with many details referencing the Art Deco movement, which inspired the name. The architectural and interiors inject elegance into a derelict building, reinstating its place as an elegant landmark of the Athenian city centre, whilst connecting the hotel to the vibrant nightlife scene surrounding it. Located inside the boundaries of the Old Historic & Commercial Center of downtown Athens, it is a great example of Greek modernist architecture of the era. The Gatsby Athens is located in the heart of the historic centre and is surrounded by buzzing bars and coffee shops so it was important for the hotel to become a central part of the neighbourhood's thriving nightlife. The adjacent alleyway has become a real feature of the hotel and a social hub for tourists and locals to meet, hang out and enjoy the neighbourhood. Covered by a metal structure with growing greenery, it links the hotel with the café opposite and also connects guests to the speakeasy 1930s style secret restaurant in the basement of the hotel.
Gatsby Athens (https://gatsbyathens.com/


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text:
Don't dis "The Sopranos," cut the homophobic trash and give Clancy a break -- readers respond to recent A&E stories
June 18, 2002 11:00PM (UTC)
[Read Laura Miller's "Sex, Death and Other Family Matters"]
I loved Laura Miller's insightful article about "Six Feet Under," but I am perplexed by the reference to "some viewers' persistent suspicion that [Rachel Griffiths' Brenda] is really more gay man than straight woman." Certainly no one would suggest that David is "more straight woman than gay man" for filling the stereotypical "unappreciated wife" role in his relationship with Keith.
It seems odd to praise (very justly) "Six Feet's" refreshingly different portrayal of gay relationships and at the same time to imply that a straight woman whose behavior conforms vaguely to certain gay stereotypes is "really" a gay man. This is the same thing I've heard about fictional women from Tennessee Williams' heroines to the gals of "Sex and the City." I'm not sure if a writer's sexuality or a female character's unconventionality is the key thing that keeps her from "really" being a woman.
We know this: Brenda was "created" by Alan Ball, a gay man. I don't know Mr. Ball, but if he's anything like every writer I've ever known, there's a little bit of himself in every character he writes about. So Brenda may "really" be a gay man in the sense that Mr. Darcy was "really" an English spinster or Count Dracula "really" a mild-mannered civil servant and theater critic. But the Brenda we see on-screen is a woman and a very believable one. (Otherwise, I'm sure Nate would have noticed.)
The days are past, at least on HBO, when gay characters and themes had to be veiled in double-entendre. Let's give these characters credit for acting as individuals first, male, female, gay, straight, black or white later, if at all. Kind of like, you know, all of us.
-- Carrie Pruett
I liked most of Laura Miller's article on the second season of "Six Feet Under," but I don't know why she felt she had to take jabs at HBO's other Sunday night powerhouse drama "The Sopranos." That show, with its phenomenal acting, writing and directing, is so much more than just a soap opera pumped up with violence so, as Miller says, "men will watch." The interpersonal relationships within the Soprano family (both literal and organizational) are every bit as complex and compelling as in the Fisher household. This is especially true of the most recent season, when all of the characters are coming face to face with the consequences of their actions and the way they have chosen to live their lives.
"Six Feet Under's" rise to "The Sopranos'" level of quality and popularity is just indicative of how good both shows are. A little love for Tony and the crew, please!
-- Clarence Ewing
[ Read Ian Rothkerch's "Holding Out for a Hero" ]
This piece is straight-up homophobic. Even more offensively, it's not funny. Bemoaning the ebb of masculine swagger is one thing, but fantasizing about the ascent of gay action heroes as some supposed part of that supposed trend takes it to another level of boneheadedness.
Next time you decide to offend, at least be smart or funny or entertaining or otherwise redeemable.
-- Michael Yarbrough
Ian Rothkerch's article was funny, but sadly the truth of real Hollywood miscasting -- casting Nick Cage as Superman in the first place comes to mind -- is still funnier.
And frankly, as a woman who thinks Connery was the only Bond worth watching, I'd trade Everett -- playing gay or straight -- for Brosnan in a heartbeat.
-- Bridgett Taylor
Please spare us expired Harvard-Lampoon rejects like "Holding Out for a Hero." If I want "The Man Show," I know where to find it.
-- Jay Winer
Ha! You almost had me with Jason Biggs (and his superstiffy) as the star of "Superman Rocks" ... but the Moby-as-Dirty-Harry remake tipped your hand. Thanks for making me laugh out loud at work. My co-workers think I'm nuts already!
-- K. Walton
Gayness = emasculation? Weak action stars are "pussies"?
Ian Rothkerch may be disgruntled with the current state of the action film industry, but surely he can express his dissatisfaction -- even satirically -- without resorting to equating perceived gayness with emasculation. And certainly a writer with his vocabulary and grasp of the English language can do better than calling these new action stars with "twice the leg power and half the charisma" pussies.
Given his dismay at what he perceives to be gay qualities, I have to assume Mr. Rothkerch is straight, which means he has devoted no small amount of time in his life trying to get some pussy himself. That he would expend so much effort to get in one (or many) and yet use "pussy" to dismiss men as inferior says a great deal about Mr. Rothkerch. I can only hope all of us pussies respond by keeping our legs closed.
-- Ashley Day
Who the f*** is this homophobic prick Ian Rothkerch, and how many references to manly, erect penises (not those disgustingly soft pussies) can this self-absorbed little asshole cram into one idiotic article?
-- Christine Curtiss
Perhaps Ian Rothkerch has never seen Matt Damon with his shirt off. It's definitely a more virile sight than hairy, barrel-chested Pierce Brosnan with that effeminate British accent.
The death of the misogynist heroes of the past, such as Han Solo, who responded to Princess Leia's professions of love with a smug "I know" is no mistake. Thank god for the end of that era. Mr. Rothkerch may long for a time when women swooned and wore lipstick and heels at home while emotionally crippled, monosyllabic men pounded their chests and put their dirty boots on the coffee table, but I certainly do not. Masculine Schmasculine. It takes a whole lot more than bravado and brute strength to impress us now.
-- Catherine Witzel
Was Ian Rothkerch's extended homophobic rant supposed to be funny? If he doubts the ability of gay men and lesbian women to kick ass, then he should keep writing articles like this for a personal demonstration.
-- Andrew Bettridge
[ Read Robert Winkler's "The Birds of Hollywood: An Unnatural History"]
Thank you for Mr. Winkler's story. As an amateur bird watcher, I've also noticed how often Hollywood uses bird songs inappropriately, especially the overuse of owl calls. Its almost a given that any movie or television program set in a rural or suburban setting will feature owl calls with every night/evening scene. Would Hollywood have us believe that every suburb in America is swarming with Owls, à la "Harry Potter"?
-- Tim De Cerbo, New Haven, Conn.
"The common loon ..." is Robert Winkler, writing in his article. What? Why? This is shamelessly obvious angling for a position as a film "bird-song" technical advisor. Mr. Winkler's article would be mildly amusing and somewhat informative if it were not filled with the strident screech of the "Show-Offs Song."
-- Catherine Oller
I'm aghast that Hollywood is chirping the wrong song. Does that mean cars don't normally explode on impact (with exception to the Ford Pinto)? Simply unbelievable! Has Hollywood been getting it wrong all these years? Please, this has to be one of the most inane articles I've ever read.
Do you know why hundreds of millions of dollars are spent on special effects? It's because it puts butts in seats in foreign markets. Nothing translates as well as unmitigated violence and explosions. Audiences have become accustomed to jaw-dropping special effects. And in Hollywood's backward thinking the bigger the explosions the bigger the box office. Besides it looks really good in a trailer.
The author's assertion that Hollywood spends millions in getting historical details right is uninformed. Is the writer an expert on all things historical? If he isn't, then how does he know these details are 100 percent accurate? The only time Hollywood toots its own horn about historical accuracy is when it's using it as a marketing ploy. "Acme studio will bring you the Revolutionary War like it really was. The horses are actual descendants from the horses used by the British!" If getting the right bird call in the background meant a bigger box office then every movie would vie for the Ornithological Society seal of approval. Getting the correct bird calls is probably pretty far down on a producer's list. It's right after making sure the production assistants are well rested and shown respect.
Phil Alden Robinson, director of "Field of Dreams," had a great comment about the authenticity problems in his movie. Ray Liotta playing the part of Shoeless Joe Jackson threw left-handed and batted right. In reality Jackson was just the opposite, batting left and throwing right. Baseball enthusiasts were up in arms. Robinson's response, did anybody realize that the character magically emerged from a cornfield? It's a movie and no one gives a hoot.
-- Jason Doty
Robert Winkler's "The Birds of Hollywood" takes anal retentiveness to a whole new level. The simple question the entire article brings up is "who cares?" Obviously Winkler does, which is a much worse reflection on him than on Hollywood.
The sounds on a movie soundtrack are meant to be evocative, to create feelings and emotions in the moviegoer. There is no law requiring that they be "accurate." Often that very "accuracy" would only ruin the effect of the film.
What's next? Complaining that, in real life, there isn't a musical soundtrack when people are going about their business? Soundtracks are by definition artificial, so complaining they are "inaccurate" is just plain silly.
Fiction does not need to be sacrificed to satisfy the great god Accuracy.
-- Chuck Rothman
Although many of Robert Winkler's points are well taken, as a birder he should know that robins frequently do sing all night long -- they are usually singing loud and clear when I rise at 2 a.m. for my annual "big day." And at least one movie, "Far North," uses bird songs that are 100 percent accurate. The sound editors of that film consulted with Bill Evans, a bird vocalization expert who was working in the Sound Library of the Cornell Laboratory of Ornithology when that movie was produced. Interestingly, many weird sounds in George Lucas films are originally inspired by bird vocalizations taken from recordings at the Cornell Laboratory of Ornithology, and digitally distorted to give them an alien quality.
I'm surprised Mr. Winkler didn't interview anyone at Cornell, which is the source of most of the bird sound recordings used in movies. It would have added a layer of depth and information to an otherwise rather superficial piece.
-- Laura Erickson
[ Read Charles Taylor's "Tom Clancy's Bogus Big-Bang Theory"]
Please. Review a movie based on the movie, not by how the advance material promoted the movie. One other thing, it's OK to be cynical, Salon has it down to an enjoyable art form. But no reason to sell your soul to being cynical at the expense of reviewing a movie whose subject matter (Salon: "the idiot government's pathetic management of an attack") you're predisposed to disliking. Was it ever possible for you to give a good review of this movie? Credibility is a virtue.
-- Stuart Sheridan
This review was as off the mark as any I have read and I am not talking about the quality of the film itself or his remarks about it as a movie. But his invective about Clancy based upon seeing him for maybe about five minutes on a news program seems puerile, and the review, in the end, seemed more about the reviewer's personal dislike of Clancy than the movie.
And it is apparent that he has not read the book, for if he had he would have understood that the original book was about Muslim nuclear terrorism, not the warmed-over U.S./Russia plot that he rightly decries.
The real question here is "Why was the plot changed?" A serious reviewer might have asked that.
-- W.J. Hunt
This article is supposedly about the movie, not about Tom Clancy, or his prescience, or lack of, in future events. I can understand attacking the movie as I remember the book did not destroy a town; in fact, it featured a nuclear bomb that failed to do much damage at all.
But in one of Tom Clancy's later books ("Debt of Honor," 1994), he had nuclear terrorists use a 747 as a missile to kill almost everyone in the government in Washington who attended the State of the Union speech. I remember right after the book was released, that some wing nut with a perceived gripe flew his small plane into the White House. Dale Brown also had commercial planes used as "bombs" as well, in his 1994 "Storming Heaven."
You may or may not like Clancy, or others of his ilk such as Dale Brown, but to disparage authors like him when they put into their fiction scenarios that turn out chillingly like real events seems like shooting the messenger, especially when it was Hollywood that the author is really railing against. Both of these authors specifically used commercial aircraft as "bombs" to destroy major buildings both outside of Washington and in Washington.
Whether or not you like Hollywood's treatment of this story, It seems to me both of these authors put holes big enough to drive a Mack truck through in the Bush administration's arguments about nobody possibly being able to call using planes as "bombs" into question on "what did Bush know, and when did he know it? The thinking was around, and I think the administration is ducking. Why is this story going away? Is Bush another "Teflon president" like Reagan, or is the press scared by Ashcroft and Cheney. Maybe the Republicans are "the guilty party"?
-- Bill Davis
[Read "Real Life Rock Top 10]
Here's what Greil Marcus might say about Greil Marcus:
"It's hard to say whether Marcus' sentences unfold or unfurl, for he's like a windshield that's been in the sun all day. And yet, for the many words and subjects and alphabet letters he crams into his reviews, the idea that they should mean something when placed next to one another seems not to give him the least bit of worry.
"Marcus seems to be saying, 'I don't know what I'm saying, but I'm going to keep writing until I reach my word count.' He's like someone who says yes out loud while shaking his head no. What does he mean by this? Casting ambivalence in concrete is like trying to apply paint to running water. His compliments hang around just long enough to turn into complaints. And he's like someone with a never-before-heard-of illness trying to describe how he feels. We want to help him, but he has to help us help him.
"To Marcus, a dense thicket of thoughts is preferable to one idea stated clearly. Sure, we can sort them out, but I can't help but think the time he saves is the time I waste trying to do so."
Or, to put it more in my own words, regarding his review of a recent Elvis Costello concert, what the hell is he talking about?
-- Jeff Hagan
Check out this article! https://www.salon.com2002/06/18/six_feet_4/


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