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

It is well known that galaxies show a wide range of morphologies, which can be appreciated
in their properties such as colour, luminosity, size, star formation histories, etc, which
imply that galaxies form and evolve through different mechanisms.
There have been many studies about the distribution of galaxies with respect to their
properties. For example, the luminosity function has been measured from various surveys of
galaxies and clusters of galaxies and it is found to be well described by the Schechter
function (\citealt{Schechter:1976}, \citealt{Loveday:1992}, \citealt{Folkes:1999},
\citealt{Mad:2002}, \citealt{Cross:2004}); the morphological types of galaxies are found
to be correlated with the environment, clusters of galaxies being the best example
(\citealt{Dressler:1980}, \citealt{Dressler:1997}, \citealt{Dominguez:2001}, \citealt{Coenda:2006}).
It is also well known that different
galaxy properties are correlated to each other. Galaxy sizes are correlated with the luminosity
and morphological type (\citealt{AP&B:1995}, \citealt{MH:2001}, \citealt{Coenda:2005},
\citealt{McI:2005}, \citealt{Trujillo:2006}), and have a distribution that may be described
by a log-normal function (\citealt{Syer:1999}, \citealt{deJL:2000}, \citealt{Shen:2003},
\citealt{Ferguson:2004}). In order to constrain the galaxy formation models and the study of galaxy
properties and their dependence on environment, we concentrate our studies on several
scaling relations and galaxy segregation.

There are different scaling relations between photometric and structural parameters of
galaxies, resulting in well known relations. One of the most established empirical scaling
relations of disk galaxies is the Tully-Fisher relation (\citealt{TF:1977}), which consist
of a correlation between luminosity and rotational velocity. The analogous relation for
spheroidal galaxies is the correlation between the velocity dispersion of bulges and luminosity,
known as the Faber-Jackson relation: $L\propto \sigma^{\beta}$ (\citealt{FJ:1976}). Other scaling
relations for spheroidal galaxies are:
color-magnitude \citep{SV:1978b,SV:1978a}, color-velocity dispersion \citep{Bernardi:2005},
radius-luminosity \citep{SP:1990} and the Kormendy relation, which is a correlation between
radius and surface brightness \citep{Kor:1977}. Some of these properties have been combined
to define the so-called \emph{fundamental plane} that relates the velocity dispersion, the effective
radius and the luminosity (\citealt{DD:1987}, \citealt{Dressler:1987}, \citealt{Bernardi:2003}).
These empirical relations are closely related to the physical processes involved in the galaxy
formation scenario and, therefore, are a fundamental tool to understand the formation and
evolution of galaxies.
These relations could depend on the environment where galaxies form and evolve, introducing
departures from scatter in the different scaling relations. Several authors have investigated
the scaling relations of galaxies in clusters. \citet{Ziegler:1999}, \citet{LaBarbera:2004}, \citet{Bernardi:2007}, \citet{vonderlinden:2007}, \citet{Liu:2007} and
\citet{Bildfell:2008}. \citet{vonderlinden:2007} found that brightest cluster galaxies
(BCG) have a higher fraction of dark matter and consequently larger radii and higher velocity
dispersions that non-BCG galaxies. \citet{Malumuth:1981,Malumuth:1985}, \citet{OH:1991} and more recently \citet{Bernardi:2007} found that BCG have
smaller $\beta$ than the rest of the cluster members. \citet{Bernardi:2007} also analyze the
dynamical mass ($M_{dyn} \propto r_{50} \sigma ^2$) and found that
BCGs show a steeper relation than non-BCG galaxies. The majority of the works mentioned
above do not make a suitable comparison with field galaxies, making it very difficult ti perform a complete
comparison of the scaling relations of galaxies as a function of the environment.
More recently, \citet{Weinmann:2009} and \citet{Guo:2009} analyzed samples of galaxies in groups and found that, at fixed stellar mass, the sizes of central
and satellite early type galaxies are similar, while \citet{Bernardi:2009}, analyzing galaxies in clusters, reported a difference at high luminosities/stellar masses between central and satellite galaxies.

It is well known that different types of galaxies show different spatial distributions
(\citealt{Oemler:1974}, \citealt{MS:1977}, \citealt{Dressler:1980}). These differences
can be estimated measuring the radial dependence of the galaxy
properties as a function of the clutocentric distance.  The segregation of galaxies in clusters has been quantified splitting galaxies
according to different properties, with
the morphology the property that has been most extensively studied, see for instance
\citet{Dressler:1980}, \citet{Whitmore:1993}, \citet{Dominguez:2001}, \citet{Biviano:2002},
\citet{Driver:2003}, \citet{Coenda:2006}. \citet{Goto:2002} found that the morphological segregation
tends to disappear for clustocentric distances larger than the virial radius. Recently, \citet{MCM:2008} found that
$g-r$ color is the property of galaxies that best predict the normalized clutocentric distance
of galaxies among a set of galaxy properties.
Similarly, \citet{Skibba:2008} used the galaxy sample of visual classified
morphologies and found that much of the morphology-density relation is due to the relation between
colour and density. The works that
have studied the segregation in luminosity present some contradictory results. \citet{RT:1968},
\citet{Yepes:1991}, \citet{Lobo:1997}, \citet{Kashi:1998}, \cite{Coenda:2006} found results consistent
with a segregation in luminosity. Nevertheless, \citet{Noonan:1961}, \citet{Bahcall:1973} and more
recently \citet{Pracy:2005} found results consistent with a lack of segregation in luminosity.
The segregation of other properties like color, star formation rate, gas content or structural
parameters have been much less studied.

The identification of clusters of galaxies is a complex process whose outcome depends on
the selection criteria. \citet{Popesso:2004} compiled X-ray clusters in the Sloan
Digital Sky Survey (SDSS).
Using the same survey, \citet{Koester:2007:alg} applied a maxBCG algorithm to
identified clusters. This technique is based on the color-magnitude relation of the early
type galaxies and the properties of the BCGs. Because we are interested in comparing the galaxy
properties of clusters selected with different criteria, the same analysis will be performed
on sub-samples of the catalogues compiled by \citet{Popesso:2004} and \citet{Koester:2007:alg}.

This paper is organised as follows: in section \ref{sec:sample} we describe the cluster and galaxy
samples; in section \ref{sec:sr} we investigate several galaxy scaling relations; in section
\ref{sec:gs} we analyze the galaxy segregation. We summarise and discuss our results in section
\ref{sec:conc}.

\section{The sample}
\label{sec:sample}

\subsection{The cluster sample}
We use two catalogues of clusters of galaxies based on the Sloan Digital
Sky Survey (SDSS; \citealt{York:2000}):
the ROSAT-SDSS Galaxy Cluster Survey of Popesso et al. (2004, hereafter P04),
which is a X-ray selected cluster sample and the MaxBGC Catalogue of Koester et al.
(2007b, hereafter K07), which is an optically selected cluster sample.

The ROSAT-SDSS catalogue of \citet{Popesso:2004} comprises 114 galaxy clusters detected in the
ROSAT All Sky Survey (RASS) lying in the area surveyed by the SDSS by February
2003. This X-ray-selected catalogue includes clusters with masses from
$10^{12.5}\cal{M}$$_{\odot}$ to $10^{15}\cal{M}$$_{\odot}$ in the redshift range
$0.002\leq z \leq 0.45$.
This catalogue provides X-ray properties of the clusters derived from the
ROSAT data, parameters of the galaxy luminosity function and the
luminosity of each cluster computed from SDSS data, and the radial
distribution of the projected galaxy density around clusters.
Since the X-ray observations provide a robust method for identifying
clusters, these clusters constitute a reliable source of information
to study galaxy properties and their correlation with the environment.

The optical MaxBGC catalogue provides sky locations, photometric redshift
estimates and richness for 13823 clusters. Details of the
selection algorithm and catalogue properties are published in
\citet{Koester:2007,Koester:2007:alg}
The MaxBGC selection relies on the observation that the galaxy population
of rich clusters is dominated by bright red galaxies tightly clustered
in colour (the E/S0 ridgeline). Since these galaxies are old, passively
evolving stellar populations, their $g-r$ colours closely reflect their
redshifts.
The brightest red galaxy, typically located at the peak of the galaxy density,
defines the cluster centre. The K07 catalogue comprises galaxy clusters with
velocity dispersions $\sigma \ge 400 \rm{km~s^{-1}}$ and redshifts $0.1\le z\le 0.3$.
Each of these clusters contains between 10 and 190 E/S0 ridgeline galaxies
brighter than $0.4L_{*}$ ($i$-band), within a scaled radius $r_{200}$
defined as the mean density of 200 times the mean density of the universe.
SDSS spectroscopic redshifts are available for at least the brightest
galaxy in $39\%$ of the clusters.  The sample is  up to $85\%$ complete
for clusters with masses $\ge 10^{14}\cal{M}$$_{\odot}$.

The sub-samples from P04 and K07 considered in this paper comprise galaxy clusters
in the redshift range $0.05<z<0.14$.
The upper limit was taken in order to have a volume limited sample of galaxies with an
adequate balance between the number of clusters, the range in absolute magnitude
and the number of cluster members.
For K07 clusters, we applied a restriction
in the richness, selecting clusters with $N_{gal}\ge 20$ in order to have cluster
masses comparable to those in the P04 sample. The sub-samples are labeled as C-P04 and C-K07
respectively. To select cluster members and estimate the physical
properties of clusters, we use the Main Galaxy Sample (MGS, \citealt{Strauss:2002})
of the Fifth Data Release (DR5) of SDSS \citep{dr5} that is complete
down to a \citet{petro76} magnitude $r=17.77$.
At this point, our sub-samples comprise 54 X-ray galaxy
clusters from the P04 sample and 612 from the K07 sample. We show in panel (a) of Figure \ref{fig:cls_z} the spectroscopic redshift distribution of 114 galaxy clusters of the P04 sample (grey solid line), the photometric redshift distribution of 13823 galaxy clusters of the K07 sample (black solid line), the distributions of those K07 clusters with $N_{gal}\ge 20$ (dotted line) and the distribution of those K07 clusters with spectroscopic redshifts (dashed line). Panel (b) shows the redshift distributions of the selected clusters C-P04 (grey line) and C-K07 (black line). We cross-correlated the catalogues to
pick clusters that are included in both of them. If the projected
distance between 2 clusters each belonging to a different catalogue
is $<1{\rm Mpc}$, we consider that they are the same cluster.
We found 20 coincidences; in these cases the clusters are only
included in the X-ray sub-sample (C-P04).

\begin{figure}
   \centering
   \includegraphics[width=9cm]{fig1.ps}
      \caption{Panal (a) shows the spectroscopic redshiht distribution of the P04 galaxy clusters (grey solid line), the photometric redshift distribution of the K07 galaxy clusters (black solid line), the distributions of those K07 clusters with $N_{gal}\ge 20$ (dotted line) and the distribution of those K07 clusters with spectroscopic redshifts (dashed line). Panel (b) shows the redshift distributions of the selected clusters C-P04 (grey line) and C-K07 (black line).}
         \label{fig:cls_z}
\end{figure}

In order to compute cluster properties such as velocity dispersion, we first
identified the cluster members. We use SDSS galaxies from the MGS
within a projected radius of $3{\rm Mpc}$ centred on the quoted cluster coordinates.
From these galaxies we identify cluster members in two steps.
First, we use the friends-of-friends (\textit{fof}) algorithm developed by
\citet{H&G:1982} with the percolation linking length values according
to \citet{Diaz:2005}. As a result, we get for each field a list of
substructures with at least 10 members identified by \textit{fof}.
The second step consists of eyeball examination of the structures
detected by \textit{fof}, a comparison between them and
the listed cluster position and redshift to determine which
coordinates and redshift fit better the observed galaxy over-density.
From the redshift distribution of galaxies within
$|cz-cz_{\rm cluster}|\le 3000\rm{km~s^{-1}}$ we determine the line-of-sight
extension of each cluster, i.e., a maximum and a minimum redshift for the
cluster. We then consider as cluster members all galaxies in the field that
are within that redshift range.
The \citet{Diaz:2005} technique includes an iterative method that provides
precise dynamical centres of the clusters.  When these centres differ from
those computed by \citet{Koester:2007}, we adopted the \textit{fof} values.
We found that for $\sim 40\%$ for the clusters, the angular position given by
the \textit{fof} is different from the original value, whereas for
$\sim 17\%$ of the clusters the redshift derived from the \textit{fof} algorithm
is a better match to the observed galaxy redshift distribution than those quoted
in the original catalogues.
Finally, we excluded from our sample those clusters for which the \textit{fof}
redshift value lay outside the redshift range we consider in this paper.

Once the members of each cluster are selected, we compute cluster physical
properties we are interested in. We compute the line-of-sight
velocity dispersion $\sigma$, the virial radius and mass and the $r_{200}$. The line-of-sight velocity dispersion $\sigma$ is estimated using
methods described by \citet{Beers:1990}. The bi-weight estimator was applied
to clusters with $\ge 15$ members, whereas the gapper estimator was applied
to poorer clusters. The radius $r_{200}$ was computed using the approximation
provided by \citet{Carlberg:1997}. In a first step,
we determined these parameters using all the cluster members within a $3{\rm Mpc}$ projected distance.
After this step, we recalculated $\sigma$ and $r_{200}$ using only
galaxies located inside $r_{200}$. Virial radis and masses were
computed following \citet{Merchan&Zandivarez:2005}.
The mean values of these parameters are shown in Table \ref{tb:mean},
where it can be seen that the sample C-P04 includes
on average clusters slightly more massive and larger than the sample
C-K07. Figure \ref{fig:hcls} shows the distributions of cluster physical
properties of our samples. The distributions of the main properties of the 20 coincident clusters are similar to those of the parent samples.

\begin{table}
\center
\begin{tabular}{ccccc}
\hline \hline
  Sample         & $\sigma$ & $R_{200}$ & $\cal{M}$$_{vir}$        & $R_{vir}$ \\
           & [$\rm{km~s^{-1}}$] & [$h^{-1} {\rm{Mpc}}$]  & [$h^{-1}\cal{M}$$_{\odot}$] &[$h^{-1} {\rm{Mpc}}$]   \\
\hline
C-P04-I & $715$    & $1.77$    & $7\times10^{14}$      & $1.75$    \\
\hline
C-K07-I & $675$    & $1.67$    & $6\times10^{14}$       & $1.59$    \\
\hline \hline
\end{tabular}
\caption{Mean values of the cluster physical properties of our cluster samples.}
\label{tb:mean}
\end{table}

Through visual inspection we classified clusters based on their
substructure. We only consider in our analysis sub-samples of regular
clusters, that we label C-P04-I and C-K07-I, and we exclude systems that have two
or more close substructures of similar size in the plane of the sky and/or in the
redshift distribution. In order to compute the physical properties in a reasonable
way, clusters with fewer than 10 galaxy members within $r_{200}$ are excluded
\citep{Girardi:1993}. Our final galaxy cluster sample comprises 49 clusters
from C-P04-I and 209 from C-K07-I.
Our sample of MaxBCG clusters is an order of magnitude smaller than the sample
considered by \citet{Bernardi:2009}, also based on the \citet{Koester:2007} catalogue. This
difference is mainly due to our restriction to select clusters with at least ten
spectroscopic members in the redshift range  $0.05<z<0.14$. The sample of \citet{Bernardi:2009} includes clusters with redshift up to 0.3 and has, on average, fewer than
one spectroscopic early-type satellite galaxy per cluster.

\begin{figure}
   \centering
   \includegraphics[width=9.2cm]{fig2.ps}
      \caption{Distributions of cluster physical properties. The
solid grey lines show the C-P04-I sample while the dashed histograms correspond to the
C-K07-I sample.}
         \label{fig:hcls}
\end{figure}

\subsection{The galaxy sample}
\label{subsec:galsample}

In order to avoid the use of weights and since we are interested in
bright galaxies, we have constructed a volume limited samples instead of a flux limited
sample. Taking into account the depth of our sample ($z<0.14$) and the apparent magnitude
limit of the Main Galaxy Sample of the SDSS, our sample of galaxies only includes objects with
$M_{^{0.1}r}<-21.3$. The C-P04-I sample comprises 786 galaxies, while the C-K07-I sample
has 3041 galaxies. Figure \ref{fig:dz} shows the redshift distributions of galaxies of our samples, C-P04-I clusters with the grey line and C-K07-I sample with the black line.
Galaxy magnitudes used throughout this paper have been corrected for galactic extinction
following \citet{sch98}, absolute magnitudes have been computed assuming
$\Omega_0=0.3$, $\Omega_{\Lambda}=0.7$ and $H_0=70~h~{\rm km~s^{-1}~Mpc^{-1}}$
and $K-$corrected using the method of \citet{Blanton:2003}~({\small KCORRECT}
version 4.1). All magnitudes are in the AB system.

Among the available data for each object in the MGS,
we have selected for our analyses parameters that are related to different
physical properties of galaxies: luminosity, star formation rate,
light distribution inside the galaxies and the dominant stellar populations.
In particular, the galaxy parameters we have focused our study on are the Petrosian $r-$band absolute
magnitude $M_{^{0.1}r}$ and the radius that encloses 50\% of the Petrosian flux $r_{50}$.
We have chosen Petrosian quantities that are not corrected for the effects of seeing. In order to reduce the effect of the PS on galaxy sizes, we excluded galaxies with $r_{50}<2''$, i.e. $0.5''$ greater than the average seeing in SDSS. This is a conservative threshold, since the PSF in SDSS is known quite accurately \citep{Shen:2003}. \citet{HydeBernandi:2009} analysed residuals from the size-luminosity relation in the SDSS Petrosian $r$-band in different redshift ranges. As expected, they found that the effect of seeing increases as a function of redshift. However, in our redshift range ($0.05<z<0.14$), these residuals are close to $0$.

Our sample consists of bright galaxies in crowded fields where SDSS reductions tend to overestimate the sky level. This results in underestimates of magnitudes and half-light radius for large half-light radii galaxies (\citealt{dr6}, \citealt{Bernardi:2007}, \citealt{HydeBernandi:2009}). In order to correct the magnitudes and sizes by sky level, we have fitted curves to SDSS simulations (DR6 documentation) and we used these fits to correct the SDSS reductions. Briefly, SDSS quantified the sky effect by adding simulated galaxies (with exponential or de Vaucouleurs) profiles to SDSS images. The simulated galaxies ranged from apparent magnitude $r=12$ to $r=19$ in half-magnitude steps, with a one-to-one mapping from $r$ to S\'ersic half-light radius (\citealt{Sersic:1963,Sersic:1968}) determined using the mean observed relation between these quantities for MGS with exponential and de Vaucouleurs profiles. Axis ratios of 0.5 and 1 were used, with random position angle for the non-circular simulated galaxies. They found a difference between the input magnitude and the model magnitude returned by the SDSS photometric pipeline, as a function of magnitude. Their results are consistent with a separate analysis performed by \citet{HydeBernandi:2009}. Finally, we have estimated the rest-frame radius $r_{50}$ in $r$-band interpolating the observed radii in the adjacent $i$-band as in \citet{HydeBernandi:2009}.

Since the aim of this work is to analyze scaling relations and segregation of different
types of galaxies in clusters and its comparison with field galaxies, we adopt several
criteria to classify galaxies. \citet{Shima:2001} found that the concentration index shows a strong
correlation with morphological type. These authors conclude that $C$ is perhaps the best
parameter to classify the morphology of galaxies. They also found that galaxies with
$R_{50}<2"$ show a weaker correlation between $C$ and the morphological type. To separate galaxies into early and late types, we use
the $r-$band concentration index defined as the ratio
between the radii that enclose 90\%  and 50\% of the Petrosian flux,
$C=r_{90}/r_{50}$. Typically, early-type galaxies have $C>2.5$, while
for late-types $C<2.5$ \citep{Strateva:2001}.
We also use the color to discriminate between early and late type galaxies. The corresponding
threshold is $^{0.1}(g-r)=0.8-0.03(M_r +20)$ (see \citet{Blanton:2007}).
Other indicator of galaxy type is the mono-parametric spectral classification based on the
eigentemplate expansion of galaxy's spectrum ${\rm eclass}$. This parameter ranges from
about $-0.35$ for early-type galaxies to $0.5$ for late-type galaxies (\citealt{Yip:2004}); the separation is set at $eclass=-0.1$. Finally, we use the S\'ersic index $n$, taken from \citet{Blanton:2005}. The distribution
of $n$ shows a bimodal distribution (see for instance \citet{Ball:2008} and \citet{Driver:2006}).
The $n$ separation is set at $2.5$, the value that divides in equal parts the two distributions and
corresponds to objects with approximately equal bulge and disk components.
In figure \ref{fig:par} we show the distributions of galaxy parameters. We can see
that clusters of the C-P04-I sample (on average, slightly more massive than C-K07-I) have a higher
fraction of red galaxies than those taken from the C-K07-I sample (89\% and 85\% respectively).

We are also interested in the study of the brightest cluster galaxies and the comparison with
early-type galaxies in both clusters and in the field. We identify the spectroscopic brightest
cluster galaxy ($BCG_s$) in our sample. The $BCG_s$ in not necessarily the true BCG due to the
following reasons: i) As a consequence of the finite fiber size of the SDSS spectrograph, any
two fibers on the same plate need to be spaced at least $55''$ apart. In the case of a fiber
collision, objects are selected at random. ii) The MSG is limited
at the bright end by the fiber magnitude limits ($r=14.5$), to avoid saturation and excessive
cross-talk in the spectrograph. These two effects together cause the spectroscopic sample to
become incomplete.

In figure \ref{fig:bcg} we show the distributions of $BCG_s$ parameters. We find that $BCG_s$
are larger and have lower surface brightness that non-$BCG_s$, in agreement with
\citet{vonderlinden:2007}. In addition, $BCG_s$ have higher velocity dispersion than non-$BCG_s$.
In general, we find that $BCG_s$ have colors, concentration and $eclass$ parameters typical of
normal early-type galaxies. Despite that $BCG_s$ are usually in the centre of the cluster
potential well, we find that the 25\% have $r/r_{200}>0.5$. Nevertheless, it is probable that a
fraction of these $BCG_s$ with large $r/r_{200}$ are not the actual BCG. It is also
possible that some of the cluster centres are wrong.
Finally, we do not find
differences between the mean properties of $BCG_s$ in the C-P04-I and C-K07-I samples.

\begin{figure}
   \centering
   \includegraphics[width=8cm]{fig3.ps}
      \caption{Redshift distributions of galaxies in our samples. Grey line: C-P04-I
sample, black line: C-K07-I sample.}
         \label{fig:dz}
\end{figure}

\begin{figure}
   \centering
   \includegraphics[width=9.3cm]{fig4.ps}
      \caption{Distributions of galaxy properties of our samples. Grey line: C-P04-I sample,
black line: C-K07-I sample.}
         \label{fig:par}
\end{figure}

\begin{figure*}
	\subfigure{\includegraphics[width=9.3cm]{fig5a.ps}}
	\subfigure{\includegraphics[width=9.3cm]{fig5b.ps}}\\
	\caption{Distributions of $BCG_s$ (dashed histograms) and $non-BCG_s$ galaxy properties of
the samples C-P04-I (left panels) and C-K07-I (right panels).}
	\label{fig:bcg}
\end{figure*}

To perform a suitable comparisson between cluster and field,
we construct a set of comparison samples. These were drawn from MGS and consist of galaxies
selected at random having the same redshift distribution as C-P04-I and C-K07-I.
This procedure excludes the cluster members.
For each cluster catalogue we have two types of samples: i) F-P04-T (52560 galaxies) and F-K07-T
(51706 galaxies) that reproduce the corresponding total redshift distribution of galaxies in clusters
and ii) F-P04-E, F-P04-L, F-K07-E and F-K07-L that reproduce the redshift distributions and
concentration index distributions of the early and late type galaxy population of C-P04-I and
C-K07-I, respectively.

\section{Scaling relations}
\label{sec:sr}

\subsection{Luminosity-size relation}
\label{ssec:lsr}

In this section we use the $r$-band concentration index $C$ to split galaxies into early and late types,
as explained in section \ref{subsec:galsample}. In Figure \ref{fig:ls} we show the
correlation between luminosity and the Petrosian half-light radius ($r_{50}\propto L^{\alpha}$). We plot the median values
of $\log(r_{50})$ versus $M_r^{0.1}$ for the C-P04-I sample (top panels) and the
C-K07-I sample (bottom panels). Error bars were obtained by the bootstrap re-sampling technique.
Slopes and zero points in this work correspond to a least-square linear regression.
The dotted lines show the $95\%$ confidence bands of the linear regressions
. Galaxies in X-ray and MaxBCG selected clusters show similar size-luminosity relations.
Early and late type galaxies (red and blue lines respectively) show clear differences, late type galaxies being larger than early types for fixed luminosities. If clusters and field galaxies
are compared, we can see in Figure \ref{fig:ls} and Table \ref{tb:lumsiz} that late type galaxies
in the field (cyan lines) are smaller than galaxies in clusters for a fix luminosity.

For early type galaxies (magenta lines), the differences between field and cluster galaxies
are also present, although, they are smaller. The effect is stronger for MaxBCG clusters. Finally,
in the common range of luminosity, $BCG_s$ (black lines) tend to be larger and show a steeper
$\log(r_{50})$ - $M_r^{0.1}$ relation than non-BCG early type galaxies in clusters.
Except for $BCG_s$, early type galaxies in clusters and in the field show the previously
reported curvature
in the size-luminosity relation (\citealt{Bernardi:2007}). For these samples of galaxies, linear
fits exclude the brightest luminosity bin.

\begin{figure*}
   \centering
   \includegraphics[width=15cm]{fig6.ps}
      \caption{The luminosity size relation: Median of $\log(r_{50})$ versus $M_r^{0.1}$
for the C-P04-I sample (top panels) and the C-K07-I sample (bottom panels). Error bars were obtained
by the bootstrap re-sampling technique. Dotted lines show the $95\%$ confidence bands of the linear
regression. The red and magenta lines show the linear regression of non-$BCG_s$ early types in cluster
and field respectively. The blue and cyan lines correspond to late types in cluster and field
respectively. Black lines show the linear fits for $BCG_s$.}
         \label{fig:ls}
\end{figure*}

We compare our results of the $r_{50}-M_r^{0.1}$ relation of BCGs with other studies. \citet{vonderlinden:2007} performed isophotal photometry from the C4 cluster catalogue (\citealt{Miller:2005}) and they found a slope $\alpha=0.65\pm 0.02$ for BCGs and $\alpha=0.63\pm 0.02$ for a control sample. \citet{Liu:2007} derived the luminosity-size relation for 85 BCGs from the same catalogue performing isophotal photometry down to four isophotal limits (22, 23, 24 and 25$\,mag\,arcsec^{-2}$); they found that the luminosity-size relation become steeper as the isophotal limit becomes fainter for both BCGs and control sample galaxies. The slope varies between $0.63\pm0.04$ and $0.88\pm0.04$ for BCGs and between $0.58\pm0.04$ and $0.74\pm0.04$ for the control sample. Although these authors used a similar photometry to \citet{vonderlinden:2007}, the difference in the slopes could be related to the differences in the brightness of the samples.
\citet{Bernardi:2007} fitted a de Vaucouleurs model to SDSS images from the C4 catalogue and used the half-light radius of their best-fitting models to study the luminosity-size relation. These authors found a slope $\alpha=0.89$. \citet{Lauer:2007} used surface photometry in HST images for 219 early type galaxies and  also fitted a de Vaucouleurs model; they found $\alpha=1.18\pm 0.06$. Once again, the photometry used in the last two works is similar but the results are very different. Again, a suitable explanation is the difference in the construction of the samples.
On the other hands, \citet{Guo:2009} used 911 central galaxies from SDSS DR4 Group catalogue (\citealt{Yang:2007}). This catalogue is constructed using the New York University Value-Addes Galaxy Catalog (\citealt{NYU}). \citet{Guo:2009} fitted a S\'ersic luminosity profile to each galaxy using GALFIT (\citealt{GALFIT}), and found a slope $\alpha=1.02\pm 0.03$ over the luminosity range $-19$ to $-24$. For galaxies brighter than $-22$, these authors found $\alpha=0.82\pm 0.06$. \citet{Shen:2003}, using spectroscopic SDSS galaxies and also S\'ersic luminosity profiles, found $\alpha=0.65$.
Recently, \citet{HydeBernandi:2009} used early-type BCGs identified in the SDSS MaxBCGS and C4 catalogs and found $\alpha=0.6$ for early-type galaxies, while BCGs follow a steeper relation.
It should be noted that the slopes resulting from our work are typically shallower than the slopes found in the different works mentioned above. Partially, these differences in slopes could be the result of the different methods used to perform the photometry. While the works mentioned above used de Vaucouleurs, isophotal or S\'ersic models, we used Petrosian magnitudes and sizes. In addition, the sample selection causes variations in the value of the slopes; for example the use or not of spectroscopic data can introduce important differences in the results, as has been demonstrated by \citet{Coenda:2006}. Beyond the differences in the slopes, it should be noted that BCGs always follow a steeper relation than galaxies in control samples.

\begin{table},
\begin{center}
\begin{tabular}{llll}
\hline \hline
          & C-P04-I         &                  &                  \\
\hline
          & \it{early non-BCGs} & \it{BCGs}    & \it{early field}    \\
\hline
$\alpha$  & $0.48\pm 0.05$  & $0.55\pm 0.08$   & $0.425\pm 0.008$  \\
$b$       & $-3.5\pm0.3$    & $-4.1\pm0.6 $    & $-3.10\pm 0.07$  \\
\hline
          & \it{late}       &                  & \it{late field}         \\
\hline
$\alpha$  & $0.4\pm 0.2$ &                     & $0.278\pm 0.005$     \\
$b$       & $-3\pm 1$       &                  & $-1.79\pm 0.04$    \\
\hline \hline
          & C-K07-I         &                  &                         \\
\hline
          & \it{early non-BCGs}     & \it{BCGs} &  \it{early field}       \\
\hline
$\alpha$  & $0.41\pm 0.02$    & $0.55\pm 0.08$ & $0.180\pm 0.003$       \\
$b$       & $-2.9\pm 0.2$     & $-4.2\pm 0.7$   & $-0.91\pm 0.03$     \\
\hline
          & \it{late}         &                 &   \it{late field}         \\
\hline
$\alpha$  & $0.40\pm 0.08$   &                  & $0.30\pm0.01$       \\
$b$       & $-2.8\pm 0.6$     &                 & $-1.88\pm0.08$      \\
\hline \hline
\end{tabular}
\end{center}
\caption{Parameter of the fits $\log(r_{50})= -0.4\alpha M_r+b$, see figure \ref{fig:ls}.}
\label{tb:lumsiz}
\end{table}

\subsection{Dynamical relations}
\label{ssec:dyn}

It is known that velocity dispersion and luminosity are well correlated for early-type galaxies
($L\propto \sigma^{\beta}$), a relation known as Faber-Jackson (\citealt{FJ:1976}).
Figure \ref{fig:fj} shows the median values of $\log{\sigma}$ as function of $M^{0.1}_r$
for early-type galaxies in clusters (red lines), control sample (magenta lines)
and $BCG_s$ (black lines). Table \ref{tb:fj} gives the parameters of the fits, where we can appreciate
that there are no differences between fits corresponding to both cluster samples.
Where we do see a clear difference is between galaxies in clusters (both $BCG_s$ and
non-$BCG_s$) and field galaxies, the latter being dynamically cooler (show lower mean velocity
dispersions). The $\log{\sigma}$-$M^{0.1}_r$ also presents a departure from linearity
for the brightest bin, where bright early type galaxies show a lower velocity dispersion than that
expected from the linear relation that fits the lower magnitude bins. $BCG_s$ show a $\log{\sigma}$-$M^{0.1}_r$ relation flatter than that of non-BCG galaxies.
Nevertheless, the mean velocity dispersion that corresponds to the brightest luminosity bin of non-BCG
galaxies is consistent with the values expected for $BCG_s$. Therefore, the flattening of the
$\log{\sigma}$-$M^{0.1}_r$ relation observed for $BCG_s$ (see also \citet{Bernardi:2007})
could be a general property of early type galaxies regardless of its nature as the brightest cluster galaxy.
\citet{Liu:2007} and \citet{vonderlinden:2007} found that BCGs have a Faber-Jackson relation steeper than that of early-type galaxies. On the contrary, \citet{Bernardi:2007} found a shallower relation for BCGs, consistent with our findings.

In Figure \ref{fig:fj} we found that early-type and $BCG_s$ galaxies
have, on average, the same velocity dispersions at a given luminosity. We also found that
$BCG_s$ have larger sizes than early type galaxies. Therefore, a different trend of dynamical
masses as a function of luminosity between these two types of galaxies should be expected. In Figure \ref{fig:ml} we show the median value of $\log(r_{50}\sigma^2)$ as a function of the luminosity for early-types, $BGG_s$ and control-sample galaxies. Again, the brightest bins show a departure from linearity and were excluded from the linear fits. For the three samples we plot a linear regression that confirm
that $BCG_s$ have, on average, higher dynamical masses than early-type galaxies of the same magnitude
(the fitting parameters are given in Table \ref{tb:ml}). It should be noted that these differences are
more significant for MaxBCG clusters (C-K07-I) than for X-ray clusters (C-P04-I). Field galaxies
in control samples show lower dynamical masses than non-BCGs in clusters.

\begin{figure*}
   \centering
   \includegraphics[width=13cm]{fig7.ps}
      \caption{Faber-Jackson Relation: Linear fits of $\log(\sigma)$ versus $M_r^{0.1}$ for
$non-BCG_s$ early-types (red lines), $BCG_s$ (black lines) and control samples (magenta lines). The panels correspond
to the same cases as in Figure \ref{fig:ls}.}
         \label{fig:fj}
\end{figure*}

\begin{figure*}
	\centering
        \includegraphics[width=13cm]{fig8.ps}
	\caption{Correlation between dynamical mass $r_{50\sigma^2}$ and luminosity for
early-types (red lines), $BCG_s$ (black lines) and control samples (magenta lines), as in Figure
\ref{fig:fj}.}
	\label{fig:ml}
\end{figure*}

\begin{table}
\begin{center}
\begin{tabular}{llll}
\hline \hline
          & \it{early non-BCGs} & \it{BCGs}      &    \it{early field}      \\
\hline
          & C-P04-I           &                  & F-P04-E  \\
\hline
$\beta$   & $4.0\pm 0.8$      & $4\pm 2$         &  $2.67\pm 0.05$  \\
$b$       & $-0.1\pm 0.3$     & $0\pm 1 $        &   $-1.03\pm 0.06$   \\
\hline \hline
          & C-K07-I           &                  & F-K07-E  \\
\hline
$\beta$   & $3.9\pm 0.2$      & $7\pm 3$         & $2.61\pm 0.05$ \\
$b$       & $0.0\pm 0.1$      & $1.0\pm 0.7$     & $-1.11\pm 0.06$    \\
\hline \hline
\end{tabular}
\end{center}
\caption{Parameters of the fits $\log(\sigma)= -\frac{0.4}{\beta}M_r+b$, see figure \ref{fig:fj}.}
\label{tb:fj}
\end{table}

\begin{table}
\begin{center}
\begin{tabular}{llll}
\hline \hline
        & \it{early non-BCGs}     & \it{BCGs}     &   \it{early field}      \\
\hline
        & C-P04-I        &                & F-P04-E  \\
\hline
$a$   & $-0.43\pm 0.03$ & $-0.5\pm 0.1$    &   $-0.464\pm 0.005$  \\
$b$   & $-4.2\pm 0.7$   & $-6\pm 2 $       &   $-5.0\pm 0.1$   \\
\hline \hline
      & C-K07-I        &                   & F-K07-E  \\
\hline
$a$   & $-0.40\pm 0.01$ &   $-0.46\pm 0.05$ & $-0.425\pm 0.005$ \\
$b$   & $-3.5\pm 0.3$     & $-5\pm 1$       & $-4.1\pm 0.1$    \\
\hline \hline
\end{tabular}
\end{center}
\caption{Parameters of the fits $\log(r_{50}\sigma^2)= aM_r+b$, see figure \ref{fig:ml}.}
\label{tb:ml}
\end{table}

\section{Galaxy segregation}
\label{sec:gs}

Using the C-P04-I and C-K07-I samples, \citet{MCM:2008} found that galaxy properties show
a clear dependence on the clustocentric distance: a higher fraction of early type galaxies
are found in the inner regions of clusters. In addition, they found that the $g-r$ colour is the
property most predictive of the clustocentric distance of galaxies. \citet{Skibba:2008} used
SDSS galaxies with data from the Galaxy Zoo (\citealt{Bamford:2008}) and found that
for fixed morphology, the environmental dependence of colour remains strong.
\citet{Blanton:2007} found that the relation between galaxy colors and
the distance from the centre of groups has a residual relationship on the clustering
of galaxies at small scales ($<300 h^{-1}$ Kpc).
In this work we are interested in the study of the segregation of several properties of bright
galaxies in clusters as a function of $r/r_{200}$ and its dependence on the cluster
identification techniques. \citet{Coenda:2006} found that these type of
analysis can produce different results depending on whether redshift-confirmed members or
galaxies in projection are considered. Although we are only considering bright galaxies, our
analysis is based on confirmed members in volume limited galaxy samples identified with two different criteria and galaxies extracted from the same galaxy catalogue.
The characteristics of these samples make them suitable for an unbiased analysis of the properties
of galaxies and its dependence on the cluster environment.

As we explained in section \ref{subsec:galsample}, we have adopted several criteria to classify galaxies
into morphological classes or types. We have used in our analysis the following parameters:
the $g-r$ colour, the concentration index $C$, the $eclass$ parameter and the Sersic index $n$.
Although they are not independent, they are dominated by different physical properties of galaxies.

Figure \ref{fig:morseg} shows the fraction of early type galaxies as a function of the
clustocentric radius. For both cluster samples a clear dependence of $r/r_{200}$ with $g-r$, $C$
and $eclass$ is found (panels a) to c)). The correlation is up to $r/r_{200} \sim 1$, for larger
clustocentric distances we do not see any tendency. For the Sersic index $n$
(panel d))
we only observe a dependence for the C-K07-I sample. The comparison between the two cluster samples
shows that the X-ray selected clusters always present a higher fraction of early type galaxies
in the whole range of clustocentric distances.
As it was pointed out previously, the X-ray sample has a slightly higher fraction of massive clusters
than the MaxBCG sample. In order to test if this difference in the mass distributions can be
responsible for the higher fraction of early type galaxies in C-P04-I than in C-K07-I sample, we
constructed a new sub-sample (C-K07-M) that consists of galaxies selected at random from C-K07-I
having the same parent-cluster mass distribution as C-P04-I. As can be appreciated in figure
\ref{fig:morseg}, the fractions of early type galaxies as a function of $r/r_{200}$ for C-K07-M
(dotted lines) are indistinguishable from those corresponding to the C-K07-I sample, indicating
that our finding of a higher fraction of early type galaxies in X-ray than in MaxBCG clusters is
independent of the dynamical mass distribution.

\begin{figure}
   \centering
   \includegraphics[width=8.5cm]{fig9.ps}
      \caption{Fraction of early type galaxies as a function of the normalized clustocentric radius.
Early type galaxies are selected according to several parameters: $(g-r)^{0.1}$ in panel (a), $C$ in
panel (b), $eclass$ in panel (c) and $n$ in panel (d). The solid grey lines show the C-P04-I sample,
whereas the solid black lines show the C-K07-I sample. The dotted black lines show the C-K07-M sample.}
         \label{fig:morseg}
\end{figure}

In panel (a) of figure \ref{fig:fm} we show the fraction of galaxies brighter than $M_r^{0.1}\le -22.5$ as a function of the normalized clustocentric distance. Analogously to the morphological segregation, we can see
a clear dependence of this fraction for $r/r_{200} \lesssim 1$, in the sense that galaxies brighter $M_r^{0.1}\le -22.5$
preferentially inhabit the cluster centres. This trend is stronger for the C-K07-I sample. Alternatively, in panel (b) we show the median values of $M_r^{0.1}$ as a function $r/r_{200}$. We observe the dependence between the median $M_r^{0.1}$ and $r/r_{200}$ for the C-K07-I sample. This effect is not observed for C-P04-I sample. The dispersion observed in mean values of $M_r^{0.1}$ (especially for C-P04-I sample) is due to the natural spread of the luminosity function.

\begin{figure}
   \centering
   \includegraphics[width=7.5cm]{fig10.ps}
      \caption{Panel (a): Fraction of galaxies brighter than $M_r^{0.1}\le -22.5$ as a function
of $r/r_{200}$. The grey line shows the C-P04-I sample while the black line corresponds to the C-K07-I sample. The horizontal dashed lines show the median values of the corresponding field samples in the same colors as their cluster counterparts. Panel (b): Median values of $M_r^{0.1}$ versus $r/r_{200}$. The horizontal lines show the median values of the corresponding field samples.}
         \label{fig:fm}
\end{figure}

\begin{figure}
   \centering
   \includegraphics[width=7.5cm]{fig11.ps}
      \caption{Panel (a) shows the median values of $r_{50}$ versus $r/r_{200}$ and panel(b) the median values of $\mu_{50}$ versus $r/r_{200}$. The horizontal lines show the median values of the corresponding field samples, as in Figure \ref{fig:fm}.}
         \label{fig:s0}
\end{figure}

\begin{figure}
   \centering
   \includegraphics[width=9.5cm]{fig12.ps}
      \caption{Median values of $r_{50}$ as a function of $r/r_{200}$ for early-type galaxies. In the
left panels we show this relation for the C-P04-I sample while C-K07-I clusters are shown on the right
panels. Early type galaxies were selected according to several parameters: $(g-r)^{0.1}$ in (a) and (b),
$C$ in (c) and (d), and $eclass$ in (e) and (f). Dotted lines show the same relation but excluding
the $BCG_s$.}
         \label{fig:s1}
\end{figure}

\begin{figure}
   \centering
   \includegraphics[width=9cm]{fig13.ps}
      \caption{Median values of $r_{50}$ as a function of $r/r_{200}$ for late-type galaxies,
analogously to figure \ref{fig:s1}.}
         \label{fig:s2}
\end{figure}

As discussed in section \ref{ssec:lsr}, the study of galaxy sizes and their relation to the
luminosity helps to understand the galaxy formation and evolution. Here we study a possible
dependence of galaxy size, $r_{50}$, as a function of $r/r_{200}$. Panel (a) in Figure \ref{fig:s0} shows the
median value of $r_{50}$ versus the normalized clustocentric distance, for the C-P04-I sample
(grey line) and for the C-K07-I sample (black line).
For clustocentric distances larger than $0.8$, mean sizes of galaxies remain almost constant, being
slightly larger for galaxies in X-ray clusters than in the MaxBCG sample, although the same effect
is observed for field galaxies (horizontal dashed lines in figure \ref{fig:s0}).
For smaller clustocentric distances, median sizes show different behaviour: for galaxies in
the C-P04-I sample, median values of $r_{50}$ decrease as $r/r_{200}$ goes to zero, whereas the
opposite behaviour is observed for galaxies in the C-K07-I sample. Panel (b) in Figure \ref{fig:s0} shows the median value of the $r-$band surface brightness $\mu_{50}$, computed inside $r_{50}$, as a function of $r/r_{200}$. For both cluster samples, $\mu_{50}$ decreases as $r/r_{200}$ goes to zero. Field galaxies have lower surface brightness (black horizontal line) than cluster members.

Figure \ref{fig:s1} repeats the previous analysis using only early type galaxies. In the
left panels we show this relation for the C-P04-I sample while C-K07-I sample are shown in the right
panels. We have also evaluated the influence of $BCG_s$ in our
results, repeating the analysis without $BCG_s$ (dotted lines).
Analogously to Figure \ref{fig:s0}, the sizes of early type galaxies increase when $r/r_{200}$
decreases in the C-K07-I sample. Nevertheless, this tendency disappears when $BCG_s$ are excluded.
On the other hand, the median values of $r_{50}$ decrease as $r/r_{200}$ goes to zero for the C-P04-I
sample; this effect is stronger when $BCG_s$ are excluded. These results clearly show an important
difference between clusters identified with different criteria. As can be appreciated in figure 3,
a higher fraction of early type galaxies is observed for the X-ray selected clusters. Consequently,
the different behaviour observed in Figure \ref{fig:s1}, could be the result of the differences
in the population of early type galaxies between the two samples. For instance, a higher fraction
of elliptical galaxies in the early type population of the X-ray selected clusters with respect to
the MaxBCG sample could produce a different behaviour in the mean sizes as a function of $r/ r_{200}$.
In order to test this possibility, we repeated the analysis of Figure \ref{fig:s1} selecting early type
galaxies with $c>3.1$. This new threshold includes a third of the early type galaxies previously
analyzed, and it will mostly select elliptical galaxies. For this sub-sample of early type galaxies,
we find the same trend observed in Figure \ref{fig:s1}, confirming that there is a dependence of the
mean sizes of early type galaxies on the cluster selection criterion. Based on a
sample of 228 elliptical galaxies in 24 clusters, \citet{Cypriano:2006} found that elliptical galaxies
in the inner regions of clusters are typically 5\% smaller than those in the outer regions. These authors
interpreted these results in terms of the tidal stripping of stars that lead to changes in the whole
structure of galaxies in the central regions of clusters.

Figure \ref{fig:s2} is the analogous of Figure \ref{fig:s1} for late-type galaxies. Although galaxies
in X-ray selected clusters show a tendency on average $r_{50}$ to be smaller towards the cluster
centers, this behaviour is not statistically significant.

\section{Discussion and conclusions}
\label{sec:conc}

We have compiled two catalogues of massive clusters of galaxies based on samples
that make use of different identification techniques: the P04 sample that comprises bright
X-ray galaxy clusters and the K07 sample, constructed
according to the properties of early-type galaxies. We selected sub-samples of galaxy clusters in
the redshift range $0.05<z<0.14$. For both samples, member galaxies are brighter that
$M_r^{0.1}=-21.3$ and were identified from a spectroscopic volume-limited sample of
the DR5-SDSS. In order to select a fair sample of clusters of galaxies we use the \textit{fof}
algorithm and an eyeball examination of each overdensity identified by \textit{fof}.
Throughout the visual inspection, we classified the clusters based on their substructure.
We only consider in our analysis regular clusters and we exclude systems that have two
or more close substructures of similar size in the plane of the sky and/or in the redshift
distribution. In addition, we have determined new positions in the plane of the sky and in
the line of sight. We found that for $\sim 40\%$ of the clusters, the angular position given
by \textit{fof} is better than the original value, whereas for $\sim 17\%$ of the clusters,
the redshift given by \textit{fof} is a better match to the observed mean redshift distribution
than the original value. Our final sample comprises $49$ X-ray selected clusters with 786
galaxies and $209$ MaxBCG clusters with 3041 galaxies. We have determined the following
physical properties of clusters: the line-of-sight velocity dispersion $\sigma$, the virial
radius and mass and $r_{200}$.

We have analyzed different scaling relations between photometric and dynamical parameters.
Bright galaxies were separated in early and late types according to several criteria. We have also
studed the segregation of galaxies analysing different properties as a function of the normalized
clustocentric distances. The main results are:
\begin{itemize}
\item Galaxies in X-ray and MaxBCG selected clusters show similar size-luminosity relations.
\item We found that each galaxy type has a different luminosity-size relation. This
implies a different mass-luminosity relation and/or a different star formation history.
\item For each luminosity bin, late type galaxies in the field have sizes smaller than their cluster counterpart.
\item The same effect is observed for early type galaxies, although the differences are smaller.
The stronger effect corresponds to galaxies in MaxBCG clusters.
\item At fixed luminosity, $BCG_s$ tend to be larger and show a steeper $\log(r_{50})$ -
$M_r^{0.1}$ relation than non-BCG early type galaxies in clusters.
\item Non-BCGs early type galaxies in clusters and in the field show the known curvature in the
size-luminosity relation.
\item The Faber-Jackson relation for early-type galaxies in clusters is the
same in X-ray and MaxBCG clusters.
\item We found a clear difference between galaxies in clusters (both $BCG_s$ and
non-BCG) and in the field, showing the later lower values of the velocity dispersion at fixed luminosity.
\item The $\log{\sigma}$-$M^{0.1}_r$ relation presents, at the bright end, a departure from
linearity. Bright early type galaxies show a lower velocity dispersion than the
expected from the linear relation at lower magnitudes.
\item  $BCG_s$ show a flatter $\log{\sigma}$-$M^{0.1}_r$ relation than non-BCG galaxies.
Nevertheless, the velocity dispersion of the brightest non-BCG galaxies are consistent with
the values expected for $BCG_s$.
\item At fixed luminosity, $BCG_s$ have, on average, higher dynamical masses than early-type
galaxies in clusters.
The difference is more significant for MaxBCG clusters than for X-ray selected clusters.
\item At fixed luminosity, field early type galaxies in the control samples show lower dynamical
masses than non-BCG
early type galaxies in clusters.
\item Using several criteria to classify galaxies into morphological classes, we found the well
know morphological segregation for both samples of clusters. The correlation is up to
$r/r_{200} \sim 1$; for larger clustocentric distances we do not see any trend.
\item For the whole range of clustocentric distances, X-ray selected clusters have a higher
fraction of early type galaxies than MaxBCG clusters.
\item  Within $r/r_{200} \sim 1$ we found a dependence of the fraction of galaxies brighter than
$M_r^{0.1}\le -22.5$ as a function of the normalized clustocentric distance. Bright galaxies preferentially
inhabit the cluster centers. This tendency is stronger for MaxBCG clusters.
\item For clustocentric distances larger than $0.8$, mean sizes of galaxies remain almost constant,
being slightly larger for galaxies in X-ray selected clusters than in the MaxBCG sample.
\item For $r/r_{200} \leq 0.8$, median sizes depend on the cluster sample.
For galaxies in X-ray selected clusters, median values of $r_{50}$ decrease as $r/r_{200}$ goes
to zero, whereas the opposite is observed for galaxies in the MaxBCG clusters.
\item For MaxBCG clusters, the sizes of early type galaxies increase as $r/r_{200}$ decreases. The
trend disappears when $BCG_s$ are excluded. On the contrary, the median value of $r_{50}$
decrease as $r/r_{200}$ goes to zero for X-ray selected clusters. The effect is stronger when
$BCG_s$ are excluded.
\end{itemize}

Early type galaxies in the field are lower, have lower velocity dispersion and have smaller virial
masses than their cluster counterpart. On the other hand, $BCG_s$ are larger and have higher values of the virial
masses than non-BCG in clusters, although the velocity dispersions are comparable. These differences
in the properties of early type galaxies in the field, in clusters and with $BCG_s$ are consistent
with the scenario where the environment plays a fundamental rol in the formation histories of
galaxies. These results suggest three different formation scenarios, $BCG_s$ being the
galaxies less affected by dissipation. Dry mergers have no energy loss mechanism, therefore the
formed galaxies are less centrally contracted with optical sizes larger than those of galaxies that
have undergone a dissipative merger (\citealt{Kormendy:1989}, \citealt{Nipoti:2003},
\citealt{Bernardi:2007}). \citet{Weinmann:2009} and \citet{Guo:2009} analyzed the size-luminosity relation of galaxies in groups, where the environmental effects are supposed to be different to those expected in clusters. These authors found the same size-luminosity relation for both central and satellite early type galaxies. The different results between galaxies in groups and clusters also support the idea that the size-luminosity relation depends on the environment.

At the same luminosity, late-type galaxies in clusters have larger sizes, and therefore lower
surface brightness than their field counterparts (control sample). This is in
agreement with the scenario of strangulation \citep{Larson:1980}, where the gas in the halo
is stripped, suppressing the supply of cold gas and therefore affecting the star formation rate and
the galaxy luminosity.

The X-ray selected sample C-P04-I is made of bright X-ray galaxy clusters, whereas the C-K07-I sample was
constructed according to the properties of early-type galaxies.
Several clusters in the C-K07-I sample should be X-ray emitters, although they would be,
on average, less X-ray luminous than C-P04-I clusters. The fact that X-ray selected
clusters show a higher fraction of early type galaxies whose sizes tend to decrease towards the cluster
center, effect that is not observed for galaxies in MaxBCG clusters, can be interpreted as possible
evidence that the hot intracluster medium is also playing a role in the evolution of early type galaxies.
Alternatively, the observed effect could be caused by differences in the clusters masses. Even though the
effects mentioned above are also present for sub-samples of C-P04-I and C-K07-I with the same virial
mass distribution, due to the usual uncertainties in the computation of these masses, we cannot discard
differences in the actual mass distributions. If this is the case, and C-P04-I clusters are on average more
massive than C-K07-I, decreases in the mean sizes of early type galaxies in X-ray selected clusters
could be the result of tidal stripping that can produce changes in the structure of galaxies
(see the results from numerical simulations of \citet{Aguilar:1986} and
observational evidences from \citet{Trujillo:2002} and \citet{Cypriano:2006}).
This difference between X-ray and MaxBCG selected clusters is an unexpected result that
should be explored in more detail.

\begin{acknowledgements}
This work has been partially supported with grants from Consejo Nacional
de Investigaciones Cient\'\i ficas y T\'ecnicas de la Rep\'ublica Argentina
(CONICET) and Secretar\'\i a de Ciencia y Tecnolog\'\i a de la Universidad
de C\'ordoba. We kindly thank Dr. H\'ector J. Mart\'inez for his helpful comments on the manuscript, which contributed to improve the present paper. VC acknowledges the guidance of Dr. Ariel Zandivarez in
the construction of the cluster sample.
\end{acknowledgements}

\bibliographystyle{aa}

redpajama_set_name: RedPajamaArXiv


In a reply from Achim on the FM4 forum, he said they were working on the ability to create "masks" -- which makes the app much more creative (and in my opinion would make certain aspects a lot easier to achieve). I suggested the ability to create non-proportional zooming (not usually done with an image itself, other than for creative purposes), but for creating those black or white "bars" that are used in the demo which appear to separate layers. With a "mask" you could just create a simple black rectangle as a common device that fills the entire screen, then just mask it to choose the area you would want to use (a horizontal or vertical bar, for example), or as a type of "black-out" cover over another layer if you needed that at a certain size.
In any case, I'd like to suggest the ability to create NOT ONLY rectangular/square masks, but ovals/circles as well? And to make it even better, to create masks of ANY shape, similar to creating a shape in Adobe Illustrator (using bezier curves)??
And to make it even better still, the ability to create COMPLEX shapes (masks). I created a slide show a long time ago using iMovie (I think it was), and I had a background photo appear to be imbedded in some title text (the font was extremely large and blocky, and the image appeared ONLY "inside" the text characters, which were being used as masks). Since the characters were "grouped" and they were complex, the image appeared inside the characters "A" and "O" and "P" (etc.) with the little inside sections of those characters letting the background of the slide show through, and the image itself only appeared within the character outlines.
It might be complicated to implement in FM4, but again it would be another creative step in keeping this app one of the best at what it does.
Thanks for the feature request! I put it on our list!


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Posts Tagged 'Opera Rara'
Posted in Architecture, Art, Classical Music, Contemporary Music, Design, Film, Opera, Photography, tagged Aftermath, Alex Prager: Silver Lake Drive, Arcola Theatre, August Sander: Men Without Masks, Banksy Greatest Hits 2002-208, Barbican Art Gallery, BBC National Orchestra & Chorus of Wales, BBC Proms, BBC Scottish SO, Britten Theatre, Christo & Jeanne-Claude, Cindy Sherman, Coast, Design Museum, Dorothea Lange: Politics of Seeing, Englefield House, Ethyl Smyth, Falstaff, Frida Kahlo: Making Herself Up, Gagosian Gallery, George Shaw, Gerard Richter, Glyndebourne Opera, Grimeborn, GSMD, Guildhall Art Gallery, Hauser & Wirth, Haydn, Hayward Gallery, Holst, Hope to Nope: Graphics & Politics 2008-18, Howard Hodgkin, Huw Watkins, ICA, In the Locked Room, Isabeau, John Hansard Gallery, Julie Becker: I must create a Master Piece to pay the rent, Kelly Richardson, L'ange de Nisada, LAZinc, Lee Bul, LPO, Mahler 8th Symphony, Mamma Mia: Here We Go Again, Michale Jackson On the Wall, Milton Court Studio Theatre, Newport Street Gallery, NPG, Opera Holland Park, Opera Rara, Parry, Pelleas & Melisande, Photographers Gallery, Ralph Vaughan Williams, Royal Academy of Art, Royal Albert Hall, Royal College of Music, Royal Opera Covent Garden, Serpentine Galleries, Shape of Light, Sir Peter Maxwell Davies, Southampton City Art Gallery, Spectra Ensemble, Spiegelasse (Mirror Alley), Spruth Magers, Summer Exhibition, Tacita Dean Landscape, Tate Britain, Tate Modern, The Boatswain's Mate, The Future Starts Here, The Great Spectacle, The Lighthouse, The Rape of Lucretia, Tom Jones, Tomma Abts, True Colours, V&A, Vanessa Winship: And Time Folds, William de Morgan, Yellow Submarine on August 1, 2018| Leave a Comment »
My respect for Tom Jones has grown significantly in recent years, largely due to his terrific blues and gospel albums, at a point in his career when he could so easily be banking money from Las Vegas shows, and his open-air concert at Englefield House in Berkshire didn't disappoint. A lovely evening, brilliantly diverse set list, a great band and excellent audience engagement combined to produce a very satisfying evening indeed.
The Royal College of Music put together an excellent double-bill of Huw Watkins' In the Locked Room and Peter Maxwell Davies' The Lighthouse. The former was interesting but the story too obtuse for me, but the latter was terrific, beautifully sung and played and thrillingly dramatic.
GSMD showcased three short operas by students on their composition course in their Milton Court Studio Theatre, performed by first year students on the opera programme. The first was an incomprehensible fantasy, the last a bit of a puzzle, but the middle a good slice of SciFi. Whatever you think of the material, all were superbly performed, though I'm not sure I liked the idea of including four scenes from three classic operas which spoilt the flow of the new for me.
I don't go to the Royal Opera much these days, but I was drawn to Falstaff by the casting of Bryn Terfel and it turned out to be a real treat – relocated to the 50's, brilliantly designed, with a faultless cast, though with their obscene top price of almost £200 I was only prepared to pay for a restricted view seat.
My first Prom was an opera, and it proved a bit of a disappointment. Pelleas & Melisande doesn't really lend itself to a concert, even semi-staged, so however good Glyndebourne Opera's singers and orchestra (the LPO) the other-worldliness it needed was something the RAH couldn't provide, so it was devoid of atmosphere and engagement. In some ways, it might have been better in concert rather than clumsy semi-staging. It reminded me of the days when I avoided opera outside the theatre altogether.
At Opera Holland Park, the UK premiere of a century old Mascagni opera, Isabeau, inspired by the Lady Godiva legend (no, she didn't!), was a real treat. Great choruses, lush orchestrations and two wonderful young leads.
Opera Rara have dug up some gems over the years, most notably Donizetti's Les martyrs. L'ange de Nisida isn't the best, but it's the world premiere of another Donizetti, 'lost' for 180 years, newly reconstructed, and sung and played brilliantly by the Royal Opera chorus and orchestra under Mark Elder, with five fine soloists, at Covent Garden. A treat.
The Arcola's annual Grimeborn Opera Festival got off to a cracking start with an intimate, intense production of Britten's The Rape of Lucretia which was so well sung and played, any opera house would be proud to have it. Our five opera 'passport' means we see them for £11 each, the best opera bargain ever!
Our second Grimeborn treat was Spectra Ensemble's production of the very underrated suffragette Ethyl Smyth's early 20th Century comic opera The Boatswain's Mate which was a delight. Great singing, but also great musicianship from a powerhouse trio of piano, violin and cello. Again, the intimacy of the even smaller studio served it well.
Mahler's 8th, the 'symphony of a thousand', belongs in the Royal Albert Hall and the 2018 Proms saw the BBC National Orchestra & Chorus of Wales plus five other choirs and eight soloists succeeded in filling it with joy. From where we sat, the acoustics weren't the best, and there seemed to be more subtlety in the second half, but thrilling stuff nonetheless.
My third visit to the Proms was a lovely evening of English music from the beginning of the 20th Century, indeed the beginning of modern English classical music, with five works by three people who knew one another – Vaughn Williams, the very underrated Parry and Holst – three of them I'd never heard before. The BBC National Orchestra and Chorus of Wales were again on top form.
My fourth Prom was another treat, with the BBC Scottish Symphony Orchestra pairing two London symphonies 120 years apart – Haydn and Vaughan Williams. The Haydn, in particular, sounded better than any other symphony of his I've heard. Great to see a full house for something without 'stars'.
It was good to see Yellow Submarine again after 50 years in a superbly restored version. The artwork is astonishing, though the story is rather naff!
Mamma Mia: Here we go again was way better than the reviews would have you believe, better than its predecessor in fact. The antidote to the hate that now pervades our lives on a regular basis.
Another of those bumper catch-up months for art.
Aftermath at Tate Britain, an exhibition of post-WWI art from Germany, France & the UK, was more historically fascinating than aesthetically appealing, though there were some great pictures. As if seeing 300 Otto Dix pictures in Chemnitz last month wasn't enough, there were 18 more here!
I don't normally like staged and posed photos, but I loved Alex Prager: Silver Lake Drive at the Photographers Gallery, a very cinematic show which included two captivating films.
Howard Hodgkin, who died last year, became a favourite artist of mine after an exhibition at the Hayward Gallery many years ago, so his final paintings at the Gagosian Gallery was essential viewing. It was more of the same, but the same is simplicity and colour.
I caught up with the Royal Academy of Art's reconfiguration and renovations in a lovely morning feast of art that started with the excellent Grayson Perry curated Summer Exhibition, which can now breathe, with the Sackler Galleries added for the prints. Then there was The Great Spectacle, a terrific exhibition covering the 250 years of the Summer Exhibition which linked the existing John Madejski Fine Rooms with the Weston Rooms in the main space. Then through a newly opened tunnel to the Burlington Gardens building for the Summer Exhibition's great (free) fun room, after which It ended on a bit of a low with Tacita Dean Landscape, which did marginally more for me than her companion exhibition at the NPG.
Shape of Light at Tate Modern examines the relationship between photography and abstract art over 100 years. Though fascinating, the photos were largely aesthetically unappealing and it all seemed a bit nerdy. Thankfully, the art was great, with the recently visited Bauhaus featuring.
South Korean artist Lee Bul's exhibition at the Hayward Gallery was full of quirky things, many involving reflections. Some individual works were excellent, but it was the impact of the whole lot that made it worthwhile, a very original riot of brightness. In the project space, Yuan Goang-Ming's video work was intriguing.
A theatrical day trip enabled me to pay a visit to the Southampton City Art Gallery. In addition to a small but impressive collection of masters, there was the terrific room showcasing the 10-picture The Perseus Story by pre-Raphaelite Edward Burne Jones, exhibitions by living artists George Shaw and Kelly Richardson and Coast, photos of the nearby coastline and seaside by the local Photographic Society. In the University's new John Hansard Gallery, a Gerard Richter exhibition proved fascinating, though I'm not his biggest fan. It's a lovely new space.
At the Guildhall Art Gallery, the William de Morgan ceramics exhibition was a delight. It tried to focus on his use of mathematics, but I couldn't get past the beauty of the pots, plates and tiles! A short walk away, it was the turn of the Barbican Art Gallery to wow with a double-bill of photographic exhibitions – American documentary photographer Dorothea Lange: Politics of Seeing, with photos taken in the Great Depression and of Japanese internment and migration, and British photographer Vanessa Winship: And Time Folds, an extraordinarily diverse range of work in which her travels in the Balkans and countries around the Black Sea captivated me most.
At Newport Street Gallery, True Colours brought together the work of Helen Breard, Sadie Laska and Boo Saville. I loved Beard's bright and colourful style, but it was rather sex obsessed, all bar one featuring explicit sexual acts. The other two did nothing for me. I'm glad it as a pop-in-while-passing visit!
At the Serpentine Galleries there was one treat and one pointless exhibition. The treat was Tomma Abts' geometric pictures in the Sackler Gallery, which surprised me by their beauty. In the main gallery, there was an exhibition showcasing the historical outdoor work using barrels of Christo & Jeanne-Claude through drawings and models, mostly of the giant Mastaba they created for the UAE. They created a smaller one for the Serpentine Lake from 1500 barrels which seemed like much ado about nothing to me. Fortunately, this year's Pavilion is lovely – from the inside. It doesn't look great until you enter and see that it's made of roof tiles with a reflective roof and water on part of the floor providing lovely images.
I would never have gone to Michael Jackson On the Wall at the NPG if I wasn't a member; £18! I certainly wouldn't call myself a fan, though I liked some of his music, and the messianic behaviour of his late career didn't sit at all comfortably with me. This exhibition of artworks of and inspired by him was however fascinating, so I was glad I did go!
At the Design Museum, a fascinating exhibition called Hope to Nope: Graphics & Politics 2008-18 about the impact of graphics on politics and protest in the last ten years, including the use of social media and movements like Occupy and #MeToo. A great idea, well executed.
Julie Becker: I must create a Master Piece to pay the Rent at the ICA is one of the worst exhibitions of recent years, and the ICA seems to be in a right old state. I blame you, Time Out. Again.
One of my wanders around Mayfair's private galleries brought rich pickings. At Hauser & Wirth, August Sander: Men Without Masks showcased the German photographer's obsessive but brilliant B&W portraits of people of the 20th Century. In their gallery next door, Spiegelgasse (Mirror Alley) was a mixed show of Swiss artists since the 1930's with some striking individual works by people I'd never heard of. Down the road at LAZinc, Banksy comes in from the streets for Greatest Hits 2002-2008, paintings and sculpture which do prove his worth. Next stop was Spruth Magers where 13 Cindy Sherman staged and posed character self-portraits, some multiples, each in an edition of just six, were valued at over $24m! They were good, but not that good!
Frida Kahlo: Making Herself Up at the V&A had some lovely paintings, a selection of her clothes that showed her unique style and fascinating biographical material, but it was too overcrowded, claustrophobic and poorly curated to really enjoy. We fared better in the more spacious, less crowded and cooler The Future Starts Here which was a fascinating peep into the future through current projects and initiatives.
The Rest of November
Posted in Art, Cabaret, Classical Music, Contemporary Music, Dance, Film, Opera, Photography, tagged Akram Khan, Alex Jennings, Anne Reid, Anselm Keifer, Barbican Curve, Barbican Hall, Benedict Cumberbatch, Boris Gudunov, Brian Eno, Britten's War Requiem, Catching Dreams, Celyn Jones, Cynthia Erivo, Damon Albarn, Daphnis et Egle, De La Soul, Erebus Ensemble, Ethan Hawke, Glare, Graham Coxon, GSMD, Handel House, Harriet Walter, Hayward Gallery, Intersteller, John Grant, Kano, Koestler Trust, La naissance d'Osiris, Late Turner, Les Arts Florissants, Les Martyrs, Linbury Studio Theatre, Lucy Parham, Mariinsky Opera, Marin Alsop, Martha Wainwright, Mass of the Children, Mike Leigh, Milton Court Concert Hall, Mirror City, Mr Turner, Nathan Amzi, National Youth Choir, Nick Holder, Nocturne, OAE, Olafur Eliasson, Opera Rara, Queen Elizabeth Hall, RAM Orchestras, Royal Academy of Art, Royal Albert Hall, Royal Festival Hall, Royal Hospital Chelsea, Sacred Monsters, Sadler's Wells Theatre, Set Fire to the Stars, Sir Mark Elder, St James Studio, St John's Smith Square, St. Nicholas, Stefan Bednarczyk, Sylvie Guillem, Tate Britain, The Cunning Peasant, The Imitation Game, Turner Prize, Union Chapel, Valerie Gergeiv, Waled Besthty, West End Recast, World Press Photo Exhibition on December 4, 2014| Leave a Comment »
West End Recast was an impulsive last-minute punt which proved a treat. The idea is that musical theatre performers sing songs they would never normally get to sing, because they're the wrong sex, colour, age etc. It was slow to take off, until Nathan Amzi gave us Cassie's Music & the Mirror from A Chorus Line! This was followed by a stunning Being Alive from Company by Cynthia Erivo (quite possible the best it's ever been sung), then a brilliant Rose's Turn (Gypsy) from Nick Holder to end the first half. The second didn't reach these heights, but there was much to enjoy.
I've always thought Damon Albarn was the best (pop) thing to come out of the 90's and has become someone, like Elvis Costello and David Byrne, who continually reinvents himself and is always open to collaboration and experimentation. Though his Royal Albert Hall show was built around his excellent new solo album, it dipped into other incarnations and included guest appearances from Blur's Graham Coxon, musicians from Mali, US hip-hop outfit De La Soul, rapper Kano and virtual recluse Brian Eno! Albarn is clearly in a very happy place and this was a very happy concert.
As her brother heads for the middle of the road, Martha Wainwright continues to do concerts that combine eccentricity, fun and beauty, showcasing her extraordinary voice and ability to inhabit her (and others) songs. This Queen Elizabeth Hall concert was good as the Union Chapel outing last August, though this time her son on stage outstayed his welcome. As one of my companions said, it's hard to concentrate on a song about a man dying of cancer when you're petrified a 5-year old might be about to electrocute himself!
I was hugely disappointed by John Grant at the Roundhouse earlier in the year, but had hoped that with an orchestra in the Royal Festival Hall he would be a lot better. Well the sound engineer was having none of that. With bass levels at painful vomit-inducing levels and the orchestra often buried in the mush of the mix, this was another disappointment. There were snatches of greatness (when the man at the back with the machines wasn't producing his electro shit) but on the whole it was great musicianship ruined by a seemingly deaf arsehole.
My first (of two) concerts in the short Mariinsky Opera residency at the Barbican Hall was the original version of Boris Gudunov. It was good but lacked the sparkle of Gergiev's work with the LSO. They seemed to be wheeling out a Mariinsky staple for the Nth time and going through the motions.
The contrast provided by the following night's OAE / Opera Rara concert version of Donizetti's Les Martyrs at the Royal Festival Hall couldn't have been bigger. An orchestra, chorus and six soloists under Sir Mark Elder, all at the the top of their game, polishing a rarely heard opera and producing a musical jewel that shone brighter than Donizetti's more popular operas. A spontaneous standing ovation is rare at such events, but not for this. Wonderful.
You can always rely on GSMD to give us a rare opera, but you don't think of Dvorak as rare – productions of his operas are, though. We only ever see one of the eleven he wrote (Rusalka) so it was good to catch his comedy, The Cunning Peasant, in an English translation relocating it to Hardy's Wessex. It's a bit derivative of Mozart's comedies and the first half didn't grab me, but the second half was great. As always at GSMD, the production values and the performances were excellent.
The ever inventive Les Arts Florissants' latest project is two short rarely performed Rameau opera-ballets, Daphnis et Egle & La naissance d'Osiris. The seven dancers, six singers and chorus of ten, all costumed, shared the bare Barbican Hall stage in front of the period ensemble, staging them as they would have been staged when they were first performed for the French Court in the eighteenth century. The stories are slight but it sounded gorgeous and this type of performance fascinating.
Glare at Covent Garden's Linbury Studio Theatre was a SciFi opera which I saw less than an hour after the SciFi film Interstellar (below) and it was less than half its length. I admired it more than I enjoyed it, but as modern opera goes, it's better than most. All four singers trained at GSMD and one, Sky Ingram, blew me away here as she had there.
It's been a privilege following the final chapter of Sylvie Guillem's career, as she transitioned from classical ballet to contemporary dance and this fourth show (for me) with Akram Khan, Sacred Monsters, at Sadler's Wells had a biographical twist. The dialogue was a surprise and the shows playfulness was both surprising and delightful. The music was great and the dancing of both mesmerising. In almost exactly six months it's the farewell show as she retires, wisely, at 50. Real class.
A second outing to the Mariinsky Opera Chorus, but this time on their own, unaccompanied, at GSMD's new Milton Court Concert Hall for a programme of secular music and folk songs. The acoustic was a bit harsh when they were at full throttle, but the singing was gorgeous and the standard of solos exceptional. If only they smiled more.
The following day, at a lunchtime concert at St. John's Smith Square, a small group of 10 singers, also unaccompanied, all young enough to be the children of the Mariinsky Chorus (!) made an equally gorgeous sound with music from both ends of a 500-year range. The Erebus Ensemble are an exciting new early music group who also tackle 20th century equivalents like Tavener and Part. Lovely.
Looking at a couple of hundred late teens / early twenties performing Britten's War Requiem at the Royal Festival Hall on Remembrance Sunday was deeply moving. 100 years ago, many of them would have been heading to the trenches and likely death. This added a poignancy to a beautifully sung and played requiem. The standards of the RAM orchestras and the National Youth Choir were astonishing and the three young soloists – a British tenor, a German Baritone & a Moldovan (former USSR) soprano, as Britten intended – were terrific. Not forgetting the excellent children's choir assembled especially for the occasion. Conductor Marin Alsop's command of it all was extraordinary.
The Chapel in the Royal Hospital Chelsea is a lovely venue for a choral concert and Rutter's Mass of the Children and Britten's St. Nicholas was a great pairing. Interval drinks in Wren's beautiful refectory and Chelsea Pensioners in their bright red uniforms greeting all adds to the occasion.
A visit to Handel House with the LSO Friends included a short recital in the room where Handel himself held them, with his composition room just next door. The soprano and harpsichordist sounded lovely and it was great to hear music in this historic room.
The fourth and last of the Composers in Love series at St. John's Concert Hall was Nocturne, a portrait of Chopin. Given the lack of letters left by him and his family, it was biographically sketchier than the others, but musically it was extraordinary and Lucy Parham converted me to Chopin, who hasn't really been on my musical radar up until now. The readers this time were Alex Jennings and Harriet Walter (subbing for Juliet Stevenson). What a lovely series this has been.
I didn't quite know what to expect from national treasure Anne Reid in cabaret (with Stefan Bednarczyk) at St. James Studio and I was delighted when it turned out to be the music of unsung musical theatre heroes Comden & Green, interspersed with the story of, and anecdotes from, their lives. Delightful & charming.
Mike Leigh's Mr. Turner has the most incredible cast, a who's who of British acting minus the 'stars' which would be guaranteed to win BAFTA's Best Ensemble award (if there was one). Turner's story is a fascinating one and Leigh's attention to detail is extraordinary. A towering achievement.
I liked Set Fire to the Stars, about Dylan Thomas' first US tour, when its American organiser had his work cut out to keep him under control. The US in the 50's looked great in B&W and the performances, particularly Celyn Jones as Dylan, were very good, but I thought the focus was too much on the US organiser and not enough on Thomas, no doubt because of the star casting of Ethan Hawke.
The Imitation Game is an even better film than I thought it would be. It moves between Alan Turing's childhood, wartime work and tragic final days and really does illuminate his story. In a terrific cast, Benedict Cumberbatch is extraordinary.
Even though I go to plays more than three hours long, films of similar length rarely hold my attention and I don't really know why. Interstellar comes in just under three hours but I was captivated throughout. So so much better than last year's Galaxy, maybe a touch too sentimental but an absolute must see.
I've seen Anselm Keifer works in galleries all over the world, but seeing them all together in the Royal Academy's retrospective exhibition was a bit overwhelming as they are virtually all dark and depressing with his brown-to-black palette. Many (but not all) are great as individual works, but together it's a different experience. His books were a revelation, but displayed in cases open at one page seemed like a lost curatorial opportunity to me.
Waled Besthty's installation at the Barbican's Curve Gallery is more impressive for its execution than its visual appeal. It's a whole year's worth of images created using the cyanotype printing process covering the whole curved wall. You have to take in the overall impact rather than the detail (unless you've got a day or two to spare). It's not the best the Curve has offered, but this space is still indispensable for innovative big scale works.
I'm afraid Mirror City at the Hayward Gallery went right over my head. Apparently, the artists are seeking 'to address the challenges, conditions and consequences of living in one of the world's busiest cities in the digital age'. Yeh…..back in the real world next door in the RFH, the annual World Press Photo Exhibition shows us what it's really like living in cities, countries, the world; a reminder of last year's events, mostly sad ones this year.
The Late Turner exhibition at Tate Britain is a riot of gorgeous colour and a great companion for Mike Leigh's film (above). It's a brilliant example of how a man in his 60's and 70's can be bursting with creativity and originality. Upstairs in the Turner Prize exhibition there isn't a painting in sight – it's all film, slides & photos – I wonder what Turner would think. I hated it. In the Turner Galleries themselves, one room has been given over to Olafur Eliasson's colour experiments where he tries to create the late Turner palette. The room contains giant circles each with their own colour range. Interesting.
Catching Dreams was the title of this year's Koestler Trust exhibition of art by offenders, secure patients and detainees at the Royal Festival Hall and it was as intriguing and inspirational as ever. This must be excellent therapy and great that their work is seen and sold in this way.

redpajama_set_name: RedPajamaCommonCrawl


text:
Q: Programmatically convert Power Point presentation to PDF in .net After searching a bit I still haven't got what I need.  I'm trying to convert various files to PDF using VB.Net and referencing various MS Office components like Word/Excel/PowerPoint as either COM objects or by using the PIA (Office Interop Assemblies).  In the end I want to use the COM method because it is version independent and that's important.
For Word and Excel I can make it work both ways.  But for PowerPoint I'm running into problems and would appreciate some suggestions.
Here's the 2 methods
COM
Dim appPP As Object = CreateObject("PowerPoint.Application")
Dim docPP As Object = appPP.Presentations.Open(strAttachmentFileName)
'2 is Microsoft.Office.Interop.PowerPoint.PpFixedFormatType.ppFixedFormatTypePDF
docPP.ExportAsFixedFormat(strNewFileName, 2)
docPP.Close()
appPP.Quit()

This method gets an error at the Export line -
Type mismatch. (Exception from HRESULT: 0x80020005 (DISP_E_TYPEMISMATCH))
PIA - this works ok
Imports Microsoft.Office.Interop
' PowerPoint requires this, to add a reference use COM - MS Office Type Library of same version as interop
Imports Microsoft.Office.Core
Dim appPP As New PowerPoint.Application
Dim docPP As PowerPoint.Presentation = appPP.Presentations.Open(strAttachmentFileName)
docPP.ExportAsFixedFormat(strNewFileName, PowerPoint.PpFixedFormatType.ppFixedFormatTypePDF)
docPP.Close()
appPP.Quit()

EDIT
Also in the COM version I tried the fully qualified version including references to the PIA and Office Core like this
docPP.ExportAsFixedFormat(strNewFileName, PowerPoint.PpFixedFormatType.ppFixedFormatTypePDF, PowerPoint.PpFixedFormatIntent.ppFixedFormatIntentScreen, MsoTriState.msoFalse, PowerPoint.PpPrintHandoutOrder.ppPrintHandoutVerticalFirst, PowerPoint.PpPrintOutputType.ppPrintOutputSlides, MsoTriState.msoFalse, Nothing, PowerPoint.PpPrintRangeType.ppPrintAll, "", False, False, False, False, False)
And it still gets the error

A: After experimenting with the COM version of the ExportAsFixedFormat I think there is a bug in the COM object.  I did find a workable solution tho
docPP.SaveAs(strNewFileName, 32)

I'm not sure what the version compatibility is on that.  I have Office 2010.

redpajama_set_name: RedPajamaStackExchange


A Cowboys fan recently tweeted at Cole Beasley his disbelief over the wide receiver not picking the Patriots. Beasley responded by challenging the notion that going to the Patriots would guarantee a championship.
Your mistake is assuming the patriots are gonna win every year.


One of the oversights in life is personal wasted energy.
This simply implies striving too often at the super-beta brain wave pattern energy or vibration is wasted energy and detrimental to your life energy and health.
The super-beta brain wave pattern energy is connected to go-getting, the marketplace and business world activity. It is also when the inner spirit gets depleted as we carry baggage that has accumulated through the striving.
Carrying baggage is when your life appears to have a pattern of problems that result in you feeling frustrated, disappointed, hurt, or when your inner critical voice says, 'what's the point' or 'not good enough' or 'nothing's going to change'! Too much striving, super-beta, will exhaust to the point where people yearn for the weekend and 'time off' to recharge their batteries.
Emotional baggage comes from regrets and resentments, unfinished experiences, past grievances. They impede your inner power, darken your perception and have in the past stuck a few labels on you and if these have not been erased your inner critic remembers and recycles energy depleting emotional baggage.
Distinguishing between past experience and present time identity is personal empowerment. Your problems are not and never have been set in stone. It is your emotional attachment to negative beliefs and thoughts that you host about yourself that your inner critic delights in defining who you are – this is emotional baggage.
This way of living, will never allow restoration and rejuvenation of your body, brain and spirit when the negative critic is present.
For your health, harmony and spiritual wellbeing you must learn in the business world, and your daily living how to appropriately engage the alpha brainwave rhythm, the rhythm of the earth's magnetic field. When you are in-tune-with, in the same rhythm as the earth you will naturally feel relaxed.
Locked in closed buildings with artificial lighting, constant temperature... continuously filtering negative background noise of air-conditioning, computers, machinery etc is not natural.
The reason city people go gardening and fishing is often not to catch a meal, they go to meditate. To find solace in silence! And for parents and our children can we role model what it is to find relief from the busy world!
When there is silence, striving ego is temporarily switched off or quiet for a little while, we adjust our thoughts upward, we see the beauty of the world as it really is and gain power to replenish our spirit. When there is silence there is time for introspection, time for the true self to connect to the flow of energy that life so plentifully provides.
Connecting to quietness brings you to your alpha and theta brain pattern energy and is nature's way of reaching the innermost place of harmony. Refreshed, you return to the world of parenting and the world or business you are better equipped to tap into deeper knowledge, understanding and better choices.
The beta brainwave energy and the super-beta brainwave energy is not wrong. It is an energy afforded us humans for the time of hunting. In business we use it for accuracy and accountability.
In the olden times of hunting and gathering we hunted, gathered, ate, conversed, connected and rested. To be a surviving species on earth, we listened to the law of nature, appropriately engaged specific brain pattern energies and took only that which sustained our self and community.
We can learn from human survival of the ages ... what did we do before the background entertainment of TV and social media, before the rush of the industrial world?
We spent time in silence and were a highly alert and aware species on earth.


text:
Q: WooCommerce: function that returns all product ID's in a particular category I think the title of the question is fairly self-explanatory, but to detail it...
I'm trying to make a custom category page in Woocommerce.
What I need is to return all the product ID's in a particular category.
I've seen this post, but it uses the WP_Query way of doing things, which is pretty ugly.
I'd prefer to use something in the WooCommerce classes to accomplish this.
Ideally, there should some sort of function/method like the following (but I can't find it):
get_products_in_category( $category_ID );
// Returns array of product ID's

Any help would be amazing.

A: Here you go:
function get_products_ids_from_category_by_id( $category_id ) {

    $products_IDs = new WP_Query( array(
        'post_type' => 'product',
        'post_status' => 'publish',
        'fields' => 'ids',
        'tax_query' => array(
            array(
                'taxonomy' => 'product_cat',
                'field' => 'term_id',
                'terms' => $category_id,
                'operator' => 'IN',
            )
        )
    ) );

    return $products_IDs;
}


On left - BomsaiBrain's 3d printed Warhammer style miniature. On right - an official GW dreadnought mini.
Anyone who's into 3d printing is probably aware that the PirateBay recently announced a new category on their torrent tracking site for 3d model files, ostensibly for 3d printing, called Physibles. Man do I have a lot to say about that.
Sartorial Printing To The Rescue!
Emergency cufflinks doing sterling duty holding my cuffs closed.
This morning, I had a bit of a wardrobe catastrophe. Nothing dramatic like a snapped thong or an impossible hairstyle – no, I couldn't find my cufflinks. Anyone who knows me knows I am both messy and forgetful – so it was only a matter of time.
So what did I do? I designed and printed a new pair before I left for work this morning.
Truly, I live in the future.


Happy New Year, everyone! Just hearing the words, "New Year," refreshes the mind. Each day, the sun rises and we celebrate the awakening of a new day. The mind and body are recharged with energy from sleep and ready to begin experiencing a new day. Even if we continue doing the same job, the same study, the same hobby, the experience is different each time, and becomes something deep.
I pray for everybody's health in 2014, and hope that you are greeted with freshness of the New Year, new experiences day-to-day, and that the year ahead will be a meaningful one for you all.


text:
Kinshasha Holman Conwill (born April 11, 1951) is a US-American museum director, arts and management consultant, author, and serves as a board member for numerous organizations within the US-American cultural sector.

Early life and education
Kinshasha Holman Conwill was born on April 11, 1951 in Atlanta, Georgia. Her parents were Mariella Ukina Ama Holman and Moses Carl Holman, the latter an editor, author, and central figure in the civil rights movement. She graduated from Mount Holyoke College in South Hadley, Massachusetts as a National Achievement Scholar.

She studied at Howard University in Washington, D.C. and received her B.F.A. in 1973. In 1980, she graduated from the University of California, Los Angeles with a M.B.A. degree.

Career
During her studies in Los Angeles, Conwill worked as an arts educator and activities coordinator for the Hollyhock House. After her graduation in 1980, she became the Deputy Director at the Studio Museum in Harlem and subsequently served as Director from 1988 until 1999. Conwill described her time at the museum and the meaning of the institution for the Black community at the occasion of their 50th anniversary:

During her time as the museum's director, they collaborated with artists such as Elizabeth Catlett, Miles Davis, Maren Hassinger, Luis Jiménez, Glenn Ligon, James Luna, Andres Serrano, James VanDerZee, and David Wojnarowicz. Furthermore, she conceptualized, organized, or co-organized more than 40 major exhibitions for the Studio Museum, some of which also travelled across the country.

Between 1999 and 2005, Conwill worked in  several positions within New York's cultural sector, among others at the American Association of Museums, the New York City Creative Communities program, the National Museum of the American Indian, the New York Foundation for the Arts, as well as the New York City Arts Coalition.

In 2005, she was appointed as deputy director of the National Museum of African American History and Culture in Washington D.C. Her role includes fundraising, external partnerships, expanding the museum's collections, and developing exhibitions and programming. She also acts as editor, author and co-author for several of the institution's publications.

Conwill has also acted as a board member for major arts and cultural organizations, such as the Provisions Library in Washington D.C., the Andy Warhol Foundation for the Visual Arts, the Municipal Art Society, and the Rockefeller Foundation.

Personal life
From 1971 until his death in 2016, Conwill was married to the artist Houston Conwill.

References

Directors of museums in the United States
Smithsonian Institution people
African-American writers
African-American museum directors
Mount Holyoke College alumni
Howard University alumni
University of California, Los Angeles alumni
Rockefeller Foundation people
1951 births
Living people

redpajama_set_name: RedPajamaWikipedia


IndePharm is a cooperative of 54 independently owned and managed pharmacies in the Republic of Ireland. Through this cooperation the members of IndePharm are working together to offer our patients and customers a choice of owner managed pharmacies which give them a convenient, high quality, efficient and cost effective range of services and products along with the highest levels of pharmaceutical care.
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Missoula, MT - Colleen passed away peacefully in her sleep at the age of 87 from Alzheimer's disease. She was born in Salem, OR to Sidney and Anita Powers. A former Queen of the Molalla Buckeroo, Colleen graduated as valedictorian from the Molalla High School. She went on to Reed College and then to Oregon State University where she graduated with a degree in early childhood education. Later she earned her Master's degree in teaching, also from OSU, and was a lifelong member of the Pi Beta Phi sorority.
She married Harold Mahon and had three children - Ann, Keith and Marlise. During their marriage, they traveled extensively throughout the US and Europe - living in Seattle, Boulder CO, Zurich, Switzerland and Newton, MA. Colleen later returned to Salem before moving to Missoula in 2013.
Colleen was an active member of the community especially with the Girl Scouts, the PTA and other causes around the family home in Newton. She worked for many years for the YWCA in Newton and Salem. She loved raising Swiss Mountain dogs and in her later years she became an avid genealogist, spending over twenty years of her life collecting photos, stories and researching the lives of her family.
She was preceded in death by her parents, and her daughter Ann Bradstreet. She is survived by her son, Keith of Stow, MA, and her daughter Marlise Flynn of Missoula; her grandchildren, Benjamin and Amalia Bradstreet, Carl, Scott and Laura Mahon and Abbey Flynn; and her former spouse, Hal.
A private family service will be held at a later date. In lieu of flowers, consider making a donation in her name to the Alzheimer's Association (www.alz.org/donate).