text:
\section{INTRODUCTION}

The properties of nearby early type galaxies (ETGs), especially the
brightest ones, offer important clues to understanding the cosmic assembly history of
massive galaxies.  In terms of their morphologies, colors, stellar
population content and scaling relations,  ETGs appear to be relatively simple
systems compared with spirals and other galaxies.
There are, however, a lot of renewed interests in their dynamical properties, particularly from the recent integral field unit surveys
(e.g. Emsellem et al. 2007; Brough et al. 2010; Cappellari et al. 2012). There is also
 a debate on their stellar mass assembly processes (Renzini 2006; Scarlata et al. 2007), and so the understanding of ETGs remains a particularly interesting issue.

In the past two decades, the concept of ``downsizing'' (Cowie et al. 1996; Gavazzi \&
Scodeggio 1996; Fontanot et al. 2009) for galaxy formation has been widely discussed. According to this scenario, the
epoch of star formation in ETGs depends on the galaxy mass, namely, the most
massive ETGs formed their stars on a shorter time scale and
at earlier times.  Furthermore, large ground-based and
space-based imaging and spectroscopic surveys at low and high redshifts
found that the mass function shows a weak evolution for massive ETGs since
redshift $\sim 1$ (e.g. Cimatti et al. 2006; Scarlata et al. 2007; Cool et al. 2008; Cimatti 2009; Vulcani et al. 2011).
In contrast, theory predicts that the typical stellar mass of most massive ETGs increases
by a factor of 2-4 since redshift one (see De Lucia \& Blaizot 2007; Tonini et al. 2012).

The size evolution for ETGs has also been the topic of many recent studies. It
has been shown that the massive and quiescent ETGs with stellar mass $M_{\ast}
\ge 10^{11}M_{\odot}$ at high redshift are more compact with effective radii a
factor of $\sim$ 3-5 smaller than the present-day ETGs with similar stellar
masses, but the stellar masses increase by a factor of $\sim$ 2 since redshift
2 (e.g. Daddi et al. 2005; Trujillo et al. 2006; van Dokkum et al. 2008).  A
popular explanation for the evolution of massive ETGs is minor dry mergers,
although additional physical mechanisms may be required (e.g. Cimatti et al.
2008; Bezanson et al. 2009; van Dokkum et al. 2010; Bruce et al.  2012 and
McLure et al. 2012). Moreoever, Valentinuzzi et al. (2010) and Poggianti
et al. (2013) found compact (superdense) massive ETGs in the local universe that have sizes
comparable to high-z massive galaxies. They argued that the evolution in
the median and average size is mild from high to low redshift for galaxies with stellar masses
$3\times 10^{10}M_{\odot} < M_{\ast} < 4\times 10^{11}M_{\odot}$, whereas the
evolution can still be substantial for ETGs more massive than $4\times 10^{11}M_{\odot}$.
It should also be noted that such studies have not
focused on the evolution of ETGs at the high mass end with $M_{\ast} \ge
10^{12}M_{\odot}$.  As pointed out by Naab (2012), the most massive ETGs or
their progenitors start forming their stars at redshift $\sim 6$ or even earlier
and these high redshift galaxies are just the cores of their local
counterparts. The assembly at later times may be inside out by accretion of
stellar mass in the outskirts of these galaxies. However, the mass assembly
history of most massive ETGs is not yet completely clear: the current
$\Lambda$CDM model cannot reproduce the stellar age, metallicity and color
evolution simultaneously (Tonini et al. 2012; De Lucia \& Borgani 2012).

To understand the mass and size evolution, accurate photometry for massive ETGs is an essential first step. Bright galaxies tend to be located in crowded environments or have extended stellar halos. Inadequate masking of their neighbors or extended halos can result in an overestimate of the
sky background, leading to an underestimate of their luminosity and size.
Indeed a number of investigators have noted that the SDSS photometric
reduction systematically underestimates the luminosities and half-light radii
for bright ETGs (see Aihara et al. 2011 for the SDSS DR8 release and
DR7 documentation). For the SDSS DR8,
a more sophisticated sky background subtraction algorithm has been adopted
and significant improvements were achieved, but some problems still persist
(see \S4.1). On the other hand, the surface brightness distribution of
most massive ETGs
cannot be fit well by a simple model such as the commonly used S\' ersic (1963) law, which can also lead to an underestimate of the luminosities.
Graham et al. (2005) carefully investigated the deficiency of
Petrosian (1976) system to quantify galaxy luminosity and size. They find that the Petrosian magnitude and size commonly used by studies based on SDSS strongly depend on the surface brightness profile.  For example, the flux deficiency can be as large as 0.5 mag for a galaxy
with $r^{1/8}$ surface brightness profile. To avoid underestimating the
luminosities of the brightest cluster galaxies (BCGs), von der Linden et al.
(2007) used isophotal photometry to 23 ${\rm mag/arcsec^2}$ in the $r$-band, rather
than the Petrosian magnitude. Therefore, aperture photometry offers a
viable alternative to describe the photometric properties of ETGs.

Underestimating the luminosities of luminous ETGs will lead to an
underestimate of the stellar mass density at the bright end. Using their
own sky background subtraction algorithm (cmodel) and  stellar mass estimation,
Bernardi et al. (2010) found a higher number of very massive galaxies than
previous works. The excess can be up to a factor of
$\sim$ 10 when the stellar mass $M_{\ast}$ is larger than $5\times 10^{11}M_{\odot}$, which is highly significant.

In this work, we perform accurate photometry for a complete
sample of nearby bright early-type galaxies with $M_{\rm r}<-22.5$ mag and
$M_\ast > 10^{11}M_{\odot}$. The morphologies of these galaxies are taken from the Galaxy Zoo project which classified nearly
900,000 SDSS galaxies (Lintott et al. 2011). We perform our own sky background subtraction, which leads to much more accurate photometry of ETGs. We then compare the
luminosities and sizes measured by different methods and investigate the
luminosity function as well as the stellar mass density for the bright ETGs.

The structure of this paper is as follows. In \S2 and \S3 we describe the sample
selection and data reduction for our bright ETGs. In \S4, we
compare our measured luminosities and sizes of bright ETGs with the SDSS Petrosian
magnitudes and sizes, and present the results of the $r$-band luminosity function
and the stellar mass density. We finish the paper with a summary in \S5. In this
paper, we adopt a Hubble constant of $H_{\rm 0}=70\,{\rm km
\, s^{-1} Mpc^{-1}}$, matter density parameter $\Omega_{m}=0.3$ and
cosmological constant $\Omega_{\Lambda}=0.7$.

\section{SAMPLE}

Our bright early type galaxy (ETG) sample is drawn from the morphological
catalogue of Galaxy Zoo 1 (Lintott et al. 2011). The Galaxy Zoo 1 project
performed visual morphological classifications for nearly 900,000 galaxies
from the Sloan Digital Sky Survey (SDSS, York et al. 2000), in which 667,945
galaxies are from the Main Galaxy Sample of SDSS (MGS, Strauss et al. 2002). The MGS
includes galaxies with $r$-band Petrosian magnitude $r\le17.77$ and $r$-band
Petrosian half-light surface brightness $\mu_{50} \le 24.5$ {\rm
mag/arcsec}$^2$. All 667,945 galaxies from the MGS have spectroscopic redshift
in the range of $0.001<z<0.25$ and u, g, r, i, z band photometry based on SDSS
DR7 (Lintott et al. 2011).

Given that the SDSS spectroscopy survey is incomplete for bright galaxies with
redshift less than 0.05 (Stoughton et al. 2002; Strauss et al. 2002; Schawinski
et al. 2007; Kaviraj et al. 2007) and reliable photometric analyses with
high signal to noise (S/N) ratios can only be performed for galaxies
with $r\le16$ mag (Fukugita et al. 2007), we constrain our bright ETG
sample to $z>0.05$ and $r<16$ mag.  Since
we are only concerned with the photometric properties of the luminous ETGs, we
further restrict our sample to bright ETGs with $M_{\rm r}<-22.5$ mag. The Petrosian absolute magnitudes, $M_{\rm r}$, are
calculated using the equation $M_{\rm r}=m_{\rm r}-5 \log(D_{\rm L}/10\,{\rm pc})-A-k$,
 where $D_{\rm L}$ is the luminosity distance,
$A$ is the Galactic extinction obtained from the photometric
catalogue of SDSS DR7 and $k$ is the k-correction derived using the IDL KCORRECT
algorithm of Blanton et al. (2007).  Finally there are 7930 bright ETGs in the
redshift range of $0.05<z<0.15$ and $M_{\rm r}<-22.5$ mag.

We further divide this sample into three volume-limited subsamples
with 2303 ETGs in the redshift ranges of $0.05<z<0.1$ for $M_{\rm r}<-22.5$
mag, 538 ETGs with $0.1<z<0.125$ for $M_{\rm r}<-23$ mag
 and 108 ETGs with $0.125<z<0.15$ for $M_{\rm r}<-23.5$ mag, as
shown in Fig.~\ref{sample-fig1}.  Then we perform $<V/V_{\rm max}>$ test (Schmidt
1968) for these subsamples.  The average value $<V/V_{\rm max}>$ are 0.51,
0.50 and 0.51 for the three subsamples, respectively, which indicates that all
the three subsamples are spatially homogeneous.
The photometric analysis in this work is based on these three subsamples.
In total, there are 2949 ETGs brighter than $-$22.5 mag, among which 1053 ETGs
are brighter than $-$23 mag.
Fig.~\ref{sky-fig2} shows the spatial distribution of our sample
galaxies on the sky in Galactic coordinates: the total area is 9055 degree$^2$,
corresponding to 22\% of the whole sky.  Fig.~\ref{histzmag-fig3} presents the
histograms showing the distributions of apparent magnitude and spectroscopic
redshift for 2949 early-type galaxies. The median Petrosian magnitude is 15.37
mag and median redshift is 0.087, respectively.

In order to verify the early-type morphology of our sample galaxies, we
visually inspected the SDSS $r$-band images for all 2949 galaxies. In
addition, we also checked other commonly used classification  criteria for
early-type galaxies.  All our sample galaxies have $g-r>0.7$
(e.g. Blanton et al. 2003; Shen et al. 2003),  and most (94\%) have
concentration index $C_{r}=r_{90}/r_{50}$ larger than 2.86 (Bernardi et al. 2010), where $r_{90}$ and $r_{50}$ are the radii containing 90\% and 50\% of Petrosian flux.
Therefore, our selected sample galaxies are all ETGs.

\section{DATA REDUCTION}

\subsection{Estimation of the Sky Background} \label{}

The corrected frame fpC-images in the $r$-band for our sample galaxies are directly
obtained from the SDSS DR7 Data Archive Server. The images have been
pre-processed by the SDSS photometric pipeline (PHOTO), which includes bias
subtraction, flat-fielding and bad pixels correction (cosmic rays removal, bad
columns and bleed trails).  In order to obtain the SDSS photometric flux
calibration information during observations, such as the photometric zeropoint
$a$, the first-order extinction coefficient $k$ and the airmass $X$, we also
downloaded the calibrated field statistic file, named as tsField from the archive.

As mentioned in \S1, the SDSS photometric reduction systematically
underestimates the luminosities and half-light radii for bright ETGs,
which is mainly caused by inadequate masking of their neighbors or extended
stellar halos (Aihara et al. 2011), leading to an overestimate of
the sky background.
In this work we perform the masking more carefully and estimate the sky background
model following Liu et al. (2008), which has been
successfully used to measure the luminosities and half-light radii for the
brightest cluster galaxies (BCGs) that are located in crowded fields and
usually have extended faint stellar halos.

In the following, we outline our sky background subtraction approach.
In order to obtain the sky background, we first masked out all objects detected
by SExtractor (Bertin \& Arounts 1996) in the corrected frames with $2048 \times 1489$ pixels ($13\arcmin.5 \times
9\arcmin.8$). We then carefully checked each frame by eye to make sure that
the wings of bright stars or the faint stellar halos of galaxies have been properly
masked. As expected, we find that the automatic algorithm of
SExtractor does not work well for about 24\% ETGs brighter than $-$22.5 mag
and 33\% ETGs brighter than $-$23 mag, which mostly include ETGs residing in crowded fields,
having extended stellar halos or are close to foreground bright stars. For the 2949 ETGs
brighter than $-$22.5 mag, the percentages of these objects are about 13\%,
7\%, 4\%, respectively. For the 1053 ETGs brighter than $-$23 mag, the
percentages are even higher, about 18\%, 10\%, 5\%, respectively. For these ETGs, we modify the mask images manually.
For comparison, Fig.~\ref{handmask-fig4} shows three cases (top, middle and bottom rows) between the
masked images generated by the automatic algorithm of SExtractor (middle
panels) and those by hand (right panels). The left panels of Fig.~\ref{handmask-fig4} show the original
true color images for the example galaxies. The top row shows a galaxy in
a crowded field.  From the top middle panel, it can be seen that SExtractor
cannot separate the target galaxy from its neighbors
well. Therefore we manually flag the nearby objects with circles that are large
enough to cover the objects completely, as shown in the top right panel.  The
second row shows a bright ETG with an
extended stellar halo.  From the middle panel, it is clear that
the flagged area generated by SExtractor is not big enough to cover the whole
stellar halo. Hence, the stellar halo would be considered as the
background and subtracted from the galaxy itself, leading to underestimates
of the luminosity and half-light radius of the galaxy.  Following the
shape of the target ETG, we use an ellipse to mask the entire stellar envelope,
as shown in the middle right panel. SExtractor also cannot handle well
galaxies surrounded by bright foreground stars, especially those
with diffractive spikes (bottom panels).  Therefore, we use long
rectangles to mask the star spikes (bottom right). The
masked images generated manually can provide not only  more accurate sky
background images but also good masks for the surface photometry (see \S 4).

To increase the valid area of the sky background subtraction, we smooth the sky background only image with a median filter of $51
\times 51$ pixels.
This filter size is selected to be larger than the sizes of most objects in the frame but still sufficiently small so that the variation of the sky background within the region is still reproduced (i.e., not smoothed out).
After the median filtering is performed, masked regions
smaller than the median box filter are replaced with the surrounding
sky background, whereas part of the masked regions larger than the median box
filter remain flagged.
With the small field of view ($13\arcmin.5 \times 9\arcmin.8$), the
  filtered sky background image is fitted with a two-dimensional first-order
Legendre polynomial (i.e., $z=a+b*x+c*y$) using the IRAF/IMSURFIT task.
The sky background map is typically tilted with a spatial variation of $\sim 1-2$ ADU across
the whole frame (Liu et al. 2008).  We subtract this
sky background model from the initial fpC-image to obtain the sky-corrected frame.
The blank regions in the sky-subtracted frame follow Gaussian distributions
with means close to zero and standard deviations of several ADU, which
is consistent with Liu et al. (2008).  After the sky subtraction, we trim both the
sky-subtracted frame and the mask image to $501 \times 501$ pixels centered on the
galaxy of interests. The trimmed mask image with the target galaxy
un-flagged will be used to probe the masked regions in the isophote fitting.

\subsection{Isophotal Photometry}

After the sky background subtraction, we perform surface photometry for our
bright ETGs in order to estimate the luminosities and sizes of sample galaxies.
As is well known, the Petrosian magnitude and Petrosian size are most commonly
used to describe the galaxy flux and half-light radius for the analyses based
on SDSS database, because they do not depend on the model fitting to galaxies.
The Petrosian radius $r_{\rm p}$ is defined as the radius $r$ at which the ratio of
the local surface brightness averaged over an annulus between $0.8r$ and
$1.25r$ to the mean surface brightness within $r$ equals to 0.2 and the
Petrosian magnitude is the integrated flux within $2r_{\rm p}$ (Petrosian 1976).
However, the Petrosian magnitude misses the light outside
$2r_{\rm p}$ (Petrosian
aperture) because of its dependence on the surface brightness profile of
galaxies (Graham et al. 2005), which leads to underestimates of the fluxes and sizes
for galaxies with extended stellar halos.  In this work, we
will measure not only the Petrosian magnitude and Petrosian half-light radius,
but also the isophotal magnitude and half-light radius to deeper
isophote limits at 25 ${\rm mag/arcsec^2}$ and 1\% of sky brightness,
corresponding to $\sim$ 26 ${\rm mag/arcsec^2}$ in most cases (Bernardi et al.
2007).

We perform the surface photometry analysis following Wu et al. (2005) and Liu
et al. (2008). The procedures are briefly described below. First, we use {\tt
ISOPHOTE/ELLIPSE} task in IRAF to fit each of the trimmed sky-subtracted images
excluding the masked regions in the fitting. The surface brightness of
the target galaxy is fitted by a series of elliptical annuli in a logarithmic
step of 0.1 along the semi-major axis. The annuli chosen in the outer
parts of image is larger, which can suppress the shot noise in the outer
regions where the signal to noise ratio (S/N) is much lower.  The output of
{\tt ISOPHOTE/ELLIPSE} is the mean intensity in each isophote annulus.  Then we
integrate the surface brightness profile to isophotal limits of 25 ${\rm
mag/arcsec^2}$ or 1\% of sky brightness to obtain the apparent
magnitudes and half-light radius $r_{50}$.  We also measure the Petrosian
magnitudes and $r_{50}$ based on our sky background subtracted
images.  In our analysis, the equivalent radius $\sqrt {ab}$ of an ellipse is
used for all the radial profiles, where $a$ and $b$ are the semi-major and
semi-minor radii of the ellipse. The cosmological dimming is also taken into
account for the surface brightness profiles.  The observational errors in the
surface brightness profile include random errors (e.g., the shot noise
of the object and sky background, readout noise and noise
contributed by data reduction) and the error from sky background subtraction.

\section{RESULTS}

\subsection{Luminosities of bright ETGs in the local universe}

The SDSS database provides the largest galaxy sample with both photometric and
spectroscopic information in the local universe. However, the underestimation
of the luminosities and sizes for the bright ETGs prevents us from
correctly understanding their properties and assembly history.

For brevity in later discussions, we define
\begin{equation}
\begin{array}{l}
\displaystyle \dmpet=m_{\rm p, \,sdss7}-m_{\rm p}, \\
\displaystyle \dmiso=m_{\rm p, \,sdss7}-m_{25},\\
\displaystyle \dmone=m_{\rm p, \,sdss7}-m_{1\%},
\label{eq:dm}
\end{array}
\end{equation}
where $m_{\rm p}$, $m_{25}$ and $m_{1\%}$ are our measured Petrosian magnitude,
isophotal magnitudes with surface brightness measured to 25 mag/arcsec$^2$ and 1\% of sky brightness,
and $m_{\rm p, \,sdss7}$ is the Petrosian magnitude from the SDSS DR7 pipeline in the $r$-band.

The top and middle panels in Fig.~\ref{1053mpetrodiff-fig5} show
$\dmpet$ (defined eq. \ref{eq:dm}) as a function of the SDSS Petrosian apparent
and absolute magnitudes, respectively, while the bottom panel shows
the histogram of $\dmpet$. Clearly for more luminous ETGs,
the luminosity difference between the SDSS and our measurements is larger.
The mean and median values of the luminosity differences are 0.16 mag and
0.14 mag, respectively. It shows that the algorithm used in the SDSS DR7 has systematically
overestimated the sky background for bright ETGs, leading to underestimates in
the luminosities of bright ETGs, especially for the brightest ones.

Addressing the same issue, in the SDSS DR8, Aihara et. al. (2011) have re-processed
all SDSS imaging data using a more sophisticated sky background subtraction
algorithm and obtained significant improvement. The left and right panels
of Fig.~\ref{comparewithdr8-fig6} are histograms of luminosity difference
 between the SDSS DR8 and SDSS DR7, and between our
measurements and SDSS DR8, respectively.  We can see
that the median values of luminosity difference for these two cases are $-$0.05 mag and $-$0.08 mag, and the mean values are about $-$0.04 mag and $-$0.12 mag, respectively.
The new algorithm on sky background subtraction used in the SDSS
DR8 has indeed improved the photometric measurement (the mean shift is about 0.04 mag). However, compared to our study it still
underestimates the luminosities by about 0.12 mag on average for bright ETGs.
We carefully checked each image with very large luminosity
differences between the SDSS DR8 and our measurements. We find that most of these
galaxies reside in crowded fields or have very extended faint stellar
halos, and so the SDSS DR8 treatment of the sky background issue is incomplete.

Liu et al. (2008) found that the isophotal magnitudes $m_{25}$ measured
to the surface brightness of 25 ${\rm mag/arcsec^2}$ are generally larger than
the Petrosian values for BCGs. We thus also compare the Petrosian and isophotal
magnitudes for our sample ETGs. The top and middle panels of
Fig.~\ref{1053misosdssdiff-fig7} show $\dmiso$ (defined in eq. \ref{eq:dm}), as a function of
the SDSS Petrosian apparent and absolute magnitudes, respectively. It is obvious that
$\dmiso$ increases with the apparent and absolute magnitudes of
ETGs. For $M_{\rm p, \,sdss7}<-23$ mag, the mean and median differences are 0.20 mag and 0.17 mag,
respectively, which are larger than those for $\dmpet$ (0.16 and 0.14 mag, respectively).

Bernardi et al. (2007) investigated the galaxy luminosity by integrating the
best-fit model of galaxy surface brightness profile to 1\% of sky
brightness.  The top and middle panels of Fig.~\ref{1053mskysdssdiff-fig8} show $\dmone$
(defined in eq. \ref{eq:dm}) as a function of
the SDSS Petrosian apparent and absolute magnitudes, respectively.
The same trend is seen: $\dmone$ increases as ETGs become more luminous.
For $M_{\rm p, \,sdss7}<-23$ mag, the mean and median values of $\dmone$ are 0.26 mag and 0.23 mag, respectively.
Note that the photometric limit of 1\% sky is $\sim$ 26 $\magsec$, almost one magnitude deeper than 25 $\magsec$.

We further examine the percentage of ETGs with large
luminosity difference between the SDSS Petrosian and our measured magnitudes. For the 2949 ETGs brighter than $-22.5$
mag, there are 6\%, 12\% and 22\%  ETGs with $\dmpet$,
$\dmiso$ and $\dmone$ larger than 0.3 mag. For the 1053
ETGs brighter than $-23$ mag, the fractions are even higher, 11\%, 19\% and 31\%, respectively.
For more luminous ETGs, the underestimation
by the SDSS algorithm is more severe. In addition, the deeper the photometric measurements, the larger the underestimations.

We point out that to the photometric limit of $\sim$ 26 ${\rm mag/arcsec^2}$
the light still belongs to galaxies as shown
by Tal \& van Dokkum (2011). They stacked more than 42000
SDSS images of LRGs (Luminous Red Galaxies), reaching a depth of $\sim$30
${\rm mag/arcsec^2}$, and found that the stellar light out to 100
kpc is physically associated with galaxies, instead of inter-cluster
or inter-group light. Our photometric measurement to 1\% sky brightness
reaches at most 100 kpc (50 kpc on average, see
\S4.2), and so our measured isophotal light is from ETGs themselves.

\subsection{Sizes of bright ETGs in the local universe}

Galaxy size is one of the most important parameters of galaxy
properties. A reliable determination of the sizes of bright ETGs in the local universe
provides the basic calibration for investigating the size evolution, an area of active study
in recent years (e.g. Szomoru et al. 2012; McLure et al. 2012;
Trujillo 2012). The aforementioned works compare galaxy sizes at high redshift to those of
the local universe by Shen et al. (2003) based on the SDSS PHOTO algorithm,
who found a power-law relation between the galaxy luminosity and size
(Shen et al. 2003). However, if the luminosities of galaxies have been
underestimated, galaxy sizes may have been underestimated too. In this section,
we will discuss the size difference between the SDSS and our measurements
based on different luminosity estimations. For convenience, we define
$r_{\rm 50, \,p}$, $r_{\rm 50, \,25}$ and $r_{\rm 50, \,1\%}$ as
our Petrosian half-light radius, isophotal half-light radii to 25 mag/arcsec$^2$ and 1\% of
the sky brightness. These values will be compared with $r_{\rm 50, \,sdss7}$, the Petrosian
half-light radius from the SDSS DR7 pipeline in the $r$-band.

Fig.~\ref{1053hist_r50-fig9} presents histograms of the half-light
radii measured by different photometric methods.
Following Shen et al. (2003), a log-normal function is fitted
to the half-light radii distribution. The log-normal function is defined as
\begin{equation}
f(r,\bar{r},\sigma_{\ln{r}})=\frac{1}{\sqrt{2\pi}\sigma_{\ln{r}}}
  \exp\left[-\frac{\ln^2(r/\bar{r})}{2\sigma_{\ln{r}}^2}\right]
  \frac{dr}{r},
\label{eq:lognormal}
\end{equation}
which is characterized by the median $\bar{r}$ and the dispersion $\sigma_{\ln{r}}$.
We find that the best-fit values for $r_{\rm 50, \,sdss7}$,
$r_{\rm 50, \,p}$, $r_{\rm 50, \,25}$, $r_{\rm 50, \,1\%}$ distributions are
$\bar{r}=8.58, 10.28, 10.80, 11.82$ kpc and $\sigma_{\ln{r}}=0.24, 0.32, 0.31, 0.32$.
From Fig.~\ref{1053hist_r50-fig9}, it can be clearly seen that the largest $r_{\rm 50, \,sdss7}$ value
is smaller than 20 kpc, while our measured $r_{\rm 50, \,p}$,
$r_{\rm 50, \,25}$ and $r_{\rm 50, \,1\%}$ can be as large as 30 kpc and
a large fraction ($\sim$ 27\%) of brightest ETGs have sizes larger than 15 kpc.
Therefore, the SDSS algorithm has significantly underestimated the real sizes of  bright ETGs.

Fig.~\ref{1053deltamag_logr50-fig10} shows the luminosity differences, $\dmpet$, $\dmiso$ and $\dmone$,
as a function of $r_{\rm 50, \, sdss7}$ respectively.
We can see from Fig.~\ref{1053deltamag_logr50-fig10} that
there is a clear trend that $\dmone$ increases as ETGs become larger.

We further examine the images of the brightest ETGs ($M_{\rm r}<-23$ mag) with
differences between the $r_{1\%}$ and the SDSS DR7 measurement larger than 10 kpc and $\dmone>0.4$ mag.
In total, there are 102 such ETGs; 56\% ETGs are in crowded field, 26\% have extended stellar halos and
the remaining 18\% are contaminated by bright nearby stars.
Fig.~\ref{image2-fig11} represents the ETGs with extended stellar halos (top
panels) and corresponding surface brightness profiles (middle panels) and the residuals
from S\' ersic models (bottom panels).
It is obvious from Fig.~\ref{image2-fig11} that the bright ETGs with such very extended stellar halos
could not be fitted well by a single S\' ersic model.

Fig.~\ref{2949logsize-luminosity-fig12} shows the size and luminosity relations
measured by different methods. In each panel, we give the best power-law fit
slope for the correlations. The top left and right panels are for Petrosian
half-light radius with Petrosian absolute magnitude obtained from the SDSS DR7
catalog and measured by us,
respectively.  The slope in the top right panel ($\alpha=0.90\pm 0.03$) is steeper than that in
the top left panel ($\alpha=0.76\pm 0.02$).  It indicates that the sky background
subtraction for bright ETGs significantly influences the size-luminosity relation.
The bottom left and right panels of Fig.~\ref{2949logsize-luminosity-fig12}
show the correlations between the size and isophotal absolute magnitude to 25
$\magsec$ and to 1\% of sky brightness, respectively.  We can see from the
bottom two panels of Fig.~\ref{2949logsize-luminosity-fig12} that the slope for
the correlation between $\log r_{50, 1\%}$ and $M_{1\%}$ ($\alpha=0.92\pm
0.03$) is somewhat steeper than the correlation between $\log r_{50, 25}$ and
$M_{25}$ ($\alpha=0.87\pm 0.02$). These results are consistent with the
size-luminosity relation trend for the brightest cluster galaxies (BCGs) obtained by
Liu et al. (2008) who found that the power-law slope becomes steeper
when the measurement goes deeper (see also Bernardi et al. 2007).

Our derived slope on the $\log r_{50}$ and $M_{\rm r}$ relation for ETGs
is much larger than the value 0.67 found by Shen at al. (2003) that
is widely adopted by recent works on the size evolution for
bright ETGs.  If we use our measured sizes of ETGs, the size evolution since redshift 2
will be somewhat larger. However, due to the surface brightness dimming, it may be difficult to perform
photometry down to 26 $\magsec$ in the rest-frame $r$-band for ETGs at
redshift 2. As a result, we should be more cautious in discussing the size
evolution by explicitly taking into account the survey surface brightness limit.

\subsection{The bright end of the $r$-band LF and stellar mass density}

A basic way to investigate galaxy properties and their
evolution is by studying the luminosity function
(LF).  There are already many LF studies using different
samples and approaches at different redshifts (see the recent
review paper by Johnston 2011). Given that the luminosities of the brightest
galaxies ($-$23.5 mag) have been underestimated (by $\sim$10\% to 40\%),
it is worth revisiting the LF at the bright end in the local universe.

In this work, we construct the galaxy luminosity function at the bright end,
utilizing the non-parametric $1/V_{\rm max}$ method (Schmidt 1968; Felten 1976; Eales 1993).
Our bright ETG sample includes 2949 galaxies consisting
of three subsamples as described in \S2, in which we have already discussed the
homogeneity for this sample. Briefly,
the $1/V_{\rm max}$ is the inverse of the maximum volume,
to which the galaxy could
have been detected. The LF is obtained by integrating $1/V_{\rm max}$ in different
luminosity bins for the whole sample of galaxies. Given that our  ETGs
contain three subsamples, we calculate the
LF in three volumes separately, and then average them to obtain the final LF.
In addition, SDSS fiber collisions lead to $\sim 7\%$ incompleteness for the
spectroscopic sample (Bernardi et al. 2010), we multiply the $1/V_{\rm max}$ counts
by a factor of $1/0.93$ to obtain the final LF.

The top panel of Fig.~\ref{2949ETGs-LF-fig13} shows our $r$-band luminosity
function at the bright end. The green triangles, red circles and blue solid squares
represent the luminosity function for our measured Petrosian magnitude,
isophotal magnitudes measured to the surface brightness
of 25 $\magsec$ and 1\% of the sky brightness, respectively.
For comparison, we also plot the luminosity
functions from Blanton et al. (2003) and Bernardi et al. (2010) in the top
panel of Fig.~\ref{2949ETGs-LF-fig13}. Blanton et al. (2003) used a
sample of 147,986 galaxies (from SDSS EDR) and
the maximum likelihood method to calculate
the luminosity function at $z=0.1$. Their sample is much larger, but includes all morphological types. However, at the
bright end  (e.g. the galaxies brighter than $-$22.5 mag), their galaxies
are almost exclusively ETGs.  The Petrosian $r$-band luminosity of galaxies
in Blanton et al. (2003) are directly
obtained from the SDSS catalogue based on the SDSS PHOTO algorithm. Bernardi et al.
(2010), on the other hand, used an ETG sample of galaxies selected from $\sim 250000$ SDSS galaxies
with $14.5<m_{\rm p, \,sdss}<17.5$ using the concentration index $C_{r}\ge2.86$,
which is a conservative way to select ETGs from SDSS.
The luminosities of ETGs in
Bernardi et al. (2010) are calculated using the cmodel in the SDSS pipeline
with their own sky background subtraction method.

It is clear from the top panel of Fig.~\ref{2949ETGs-LF-fig13} that at the bright
end  ($M_{\rm r}< -22.5$ mag), the slope of the Bernardi et al. (2010)'s LF is
shallower than that of Blanton et al. (2003), implying that the luminosity
estimation method of Bernardi et al. (2010) is a
significant improvement over the SDSS PHOTO algorithm.
However, our luminosity function of ETGs at the bright end
is even shallower, particularly when we use the photometry to 1\% of the sky brightness.

Table 1 lists our measured luminosity densities for the Petrosian magnitudes and isophotal magnitudes
to surface brightness of 25 ${\rm mag/arcsec^2}$ and 1\% of the sky background (denoted by $\phi_{\rm p}$,
$\phi_{\rm 25}$ and $\phi_{\rm 1\%}$, respectively) at several $r$-band luminosities. The
bottom panel of Fig.~\ref{2949ETGs-LF-fig13} shows the ratios of these galaxy luminosity
densities to that measured by Blanton et al. (2003), denoted as $\phiPB$,
 as a function of $r$-band luminosities. It is clear that the luminosity density ratios increase with the luminosity of ETGs. For ETGs with
 $M_{\rm r}=-$23.5 mag, the ratios are $6.7\pm0.46$, $8.0\pm0.40$ and $10.5\pm0.56$,
respectively; for ETGs with $M_{\rm r}=-$24 mag, they go
up to $153\pm14$, $197\pm16$ and $259\pm22$, respectively. It demonstrates that the luminosity
density of the brightest ETG calculated based on the SDSS catalogue has been
seriously underestimated.
Note that for the three magnitudes $M_{\rm p}$, $M_{\rm 25}$ and $M_{\rm 1\%}$,
 the number of ETGs brighter than $-$23.5 mag is 347, 385 and 486,
while the number of ETGs brighter than $-$24 mag is 41, 56 and 90,
and so the number statistics are reasonably good.
The underestimates in the luminosity density result in a significant underestimate of the integrated
luminosity density. In particular, the integrated luminosity density down to $M_{\rm r}<-22.5$ mag based
on our measured $M_{\rm p}$, $M_{25}$, $M_{1\%}$ are about 20\%, 40\%, 50\% higher than that from the SDSS Petrosian luminosity, respectively.

Next we estimate the stellar mass $M_{\ast}$ of the ETGs following Bernardi et al. (2010), utilizing the equation
\begin{equation}
\log \,M_{\ast}/M_{\odot} =
1.097(g-r)-0.406-0.4(M_{\rm r}-4.67)-0.19z,
\end{equation}
where $M_{\ast}$ is the stellar mass (in solar units), $g-r$ is the
rest-frame color, $M_{\rm r}$ is the absolute magnitude, and $z$ is the
redshift.  This equation has already taken into account the k-correction and
evolution correction, and the initial mass function (IMF) is assumed to be of
the Chabrier (2003) form (see \S2.4 of Bernardi et al. 2010 for more details).
The first two terms on the right side of eq. (3) were initially derived by Bell
et al. (2003) based on SDSS Petrosian $g-r$ color and $r$-band Petrosian
magnigtude, which have been adapted to the Chabrier IMF here. A proper model fitting to colors and
magnitudes measured using our photometric methods may give different
coefficients in eq. (3).  However, to facilitate comparison with the stellar mass function obtained by
Bernardi et al. (2010), we use the same equation as their study. Under the
assumption that the impact of our photometric algorithm on the $r$-band
photometry is the same as that on the $g$-band, we use the SDSS model $g-r$ color as
a surrogate of colors measured by our methods\footnote{In the SDSS
Data Release 2 paper (Abazajian et al. 2004) and SDSS web page, model magnitudes are recommended
to be used for the measures of the colors of extended objects.}. The stellar masses $M_{\ast,
\rm \,p}$, $M_{\ast, \,25}$ and $M_{\ast, \,1\%}$ are obtained using our
measured luminosities $M_{\rm p}$, $M_{\rm 25}$, $M_{\rm 1\%}$, respectively.

Table 2 gives the stellar mass densities, $\phi_{M_\ast, \rm \,p}$, $\phi_{M_\ast, \,25}$ and
$\phi_{M_\ast, \,1\%}$ at several stellar masses of ETGs for our measured magnitudes.
The top panel of Fig.~\ref{2949ETG-MF-fig14} shows the stellar mass function
for massive ETGs. We also plot the stellar mass function
from Blanton \& Roweis (2007) and Bernardi et al. (2010) in the top panel of
Fig.~\ref{2949ETG-MF-fig14} for comparison. As can be seen,
 the slope of our measured stellar mass functions is shallower than those
of Bernardi et al. (2010) and Blanton \& Roweis (2007).
Given that Bernardi et al. (2010) have already compared their stellar mass density with previous
observational results, in the bottom panel of Fig.~\ref{2949ETG-MF-fig14} we just compare our result with Bernardi et al. (2010).
It shows that the stellar mass densities ratios of our measurements to that of Bernardi et al. (2010), written as $\phi_{M_*, \rm \,Bernardi}$, as a function of stellar mass.
We can see from the bottom panel of Fig.~\ref{2949ETG-MF-fig14} that
the ratios are larger for more massive ETGs.
The ratios, $\phi_{M_*, \rm \,p}/\phi_{M_*, \rm \,Bernardi}$,
$\phi_{M_*, \,25}/\phi_{M_*, \rm \,Bernardi}$ and $\phi_{M_*, \,1\%}/\phi_{M_*, \rm \,Bernardi}$
are 1.2$\pm$0.06, 1.3$\pm$0.07 and 1.6$\pm$0.07 for ETGs with
$M_{\ast}\sim 5\times10^{11} M_{\odot}$; for $M_{\ast}\sim 10^{12}
M_{\odot}$, the ratios are even larger, 2.1$\pm$0.40, 2.8$\pm$0.43 and
4.2$\pm$0.58, respectively. Thus, at the high mass end the stellar mass densities have been underestimated by all previous works.

We also plot the predicted stellar mass function by Guo et al. (2011) in the top panel of
Fig.~\ref{2949ETG-MF-fig14}. Their result is based on the semi-analytic models of the galaxy population using the dark matter only Millennium Simulation. We can see that the high-mass tail of
their stellar mass function slightly over-predicts the abundance in Bernardi et al. (2010), but still
under-predicts our mass function. We return to this briefly in the next section.

\section{SUMMARY}

In this work, we performed photometric analyses for a complete and homogeneous
bright ETGs sample with 2949 early-type galaxies ($M_{\rm r}<-22.5$ mag) in the
redshift range of 0.05 to 0.15, taken from the catalog of SDSS DR7; all these
galaxies have morphological classifications from the Galaxy Zoo 1 MGS.
Based on our own sky background subtraction method, we
measured the Petrosian and isophotal magnitudes, as well as
the corresponding half-light radii. Comparing our measured luminosities and
sizes to those from SDSS, we find that the SDSS pipeline
significantly underestimates the luminosities and sizes for the brightest ETGs,
leading to underestimates of the luminosity density and stellar
mass density for bright ETGs. Our main results are summarized as
follows.

\begin{enumerate}
\item We find that for brightest galaxies ($M_{\rm}<-23$ mag),
our Petrosian magnitudes, and isophotal magnitudes to
25 ${\rm mag/arcsec^2}$ and 1\% of the sky brightness are on
average 0.16 mag, 0.20 mag, and 0.26 mag brighter than the SDSS Petrosian values, respectively.
In the first case the underestimations are due to overestimations in the sky
background by the SDSS PHOTO algorithm, while the latter two are also caused by
an additional effect of reaching deeper photometry.
Such underestimation is more severe as ETGs become more luminous. Our results also demonstrate that as
we integrate to deeper surface brightness, we recover more luminosity of galaxies.
\item We also find that the sizes of ETGs (half-light radius $r_{50}$) measured by the SDSS algorithm are smaller than those measured by us.
The largest $r_{50}$ of bright ETGs in the SDSS catalogue is $\sim$ 20 kpc, while our measured $r_{50}$ can be as large as
30 kpc and for a large fraction ($\sim$ 27\%) of brightest ETGs, $r_{50}$ is larger than 15 kpc.
In addition, we find that the slope in the size-luminosity relation at the bright end is much steeper than that
found by Shen et al. (2003).
\item Based on our selected complete and homogeneous sample of 2949 bright early-type galaxies,
we construct the luminosity function. We find that the LF at the bright end is
much shallower than those of Blanton et al. (2003) and Bernardi et al. (2010).
The luminosity density at $-$23.5 mag ($-$24 mag) measured in this work is one order (two orders) of magnitude higher than
that of Blanton et al. (2003).
As a result, the ratios of the integrated luminosity density for bright
galaxies ($M_{\rm r}<-22.5$ mag) between those based on our measured
$M_{\rm p}$, $M_{25}$, $M_{1\%}$ and the SDSS Petrosian luminosity are 1.2, 1.4 and 1.5, respectively.
Similarly, the stellar mass density of ETGs is a few tenths to a factor of few higher than that
of Bernardi et al. (2010) for stellar mass from $\sim 5\times10^{11} M_{\odot}$ to $\sim 10^{12} M_{\odot}$.
Therefore, our method recovers substantially more luminosity for bright ETGs, which
may alleviate the contradiction between hierarchical galaxy formation theories and current observations.
\end{enumerate}
Our results suggest that very careful photometry needs to be performed to
obtain the LF at the bright end which has significant impact on the
stellar mass function for massive galaxies. Previous claims that the
massive end of the stellar mass function has a weak evolution since
redshift $\sim$ 1 in comparison with the Galaxy And Mass Assembly (GAMA)
survey (Baldry et al. 2012) may need to be re-examined. Furthermore,
semi-analytical models may need to increase their cooling efficiency or
decrease the AGN feedback efficiency for massive galaxies in order to
match the shallower LF we found here. How does this affect the overall
shape of the LF (especially around $L_*$) is unclear and warrants
further studies.
Finally, we notice that recent studies on the environmental
dependence of galaxy mass function have suggested that the stellar mass
function is much more dependent on local galaxy density than global
environments of galaxies and the most massive galaxies are only located in the highest density regions (e.g. Vulcani et al. 2012; Calvi et al. 2013).
Given our finding that massive galaxies, which
are preferentially found in crowded environments, can be significantly
underestimated in their luminosity/mass due to inaccurate photometry,
the observed environmental dependence of the high-mass end of mass
function may be somehow affected by such photometry issue also.
It is worth revisiting this issue in a future work.

\acknowledgements
We thank Drs. J. S. Huang, F. S. Liu, Z. H. Shang, Qi Guo, H. J. Yan and C. G. Shu for advice and helpful discussions.
This project is supported by the NSF of China 10973011, 10833006, 11003015, the Chinese Academy of Sciences and NAOC (SM).
YPJ is supported by NSFC (11033006, 11121062) and the CAS/SAFEA International Partnership Program for Creative Research Teams (KJCX2-YW-T23).
Funding for the creation and distribution of the SDSS Archive has been provided
by the Alfred P. Sloan Foundation, the Participating Institutions, the National
Aeronautics and Space Administration, the National Science Foundation, the U.S. Department of Energy,
the Japanese Monbukagakusho, and the Max Planck Society. The SDSS Web site is http://www.sdss.org/.
The SDSS is managed by the Astrophysical Research Consortium (ARC) for the
Participating Institutions. The Participating Institutions are The University
of Chicago, Fermilab, the Institute for Advanced Study, the Japan Participation
Group, The Johns Hopkins University, the Korean Scientist Group, Los Alamos
National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the
Max-Planck-Institute for Astrophysics (MPA), New Mexico State University,
University of Pittsburgh, Princeton University, the United States Naval Observatory,
and the University of Washington.

redpajama_set_name: RedPajamaArXiv


text:
What are the functions of operating system class 11?
1 What are the functions of operating system class 11?
2 What are the functions of an operating system explain?
3 What are the 4 functions of operating system?
4 What are the 5 main functions of an operating system?
5 What are the 10 functions of operating system?
6 What are the three main functions of operating system?
7 What are the functions of the operating system PDF?
8 What is the function of an operating system Mcq?
9 What is operating system and its functions and types PPT?
10 What are the functions of operating system class 9?
Important functions of an operating System:
Security – …
Control over system performance – …
Job accounting – …
Error detecting aids – …
Coordination between other software and users – …
Memory Management – …
Processor Management – …
Device Management –
What are the functions of an operating system explain?
An operating system has three main functions: (1) manage the computer's resources, such as the central processing unit, memory, disk drives, and printers, (2) establish a user interface, and (3) execute and provide services for applications software.
What are the 4 functions of operating system?
Operating system functions Organises the use of memory between programs. Organises processing time between programs and users. Maintains security and access rights of users. Deals with errors and user instructions.
What are the 5 main functions of an operating system?
5 Key Functions of Operating System
User Interface: User interface is such a part of an operating system that creates a platform for users and other applications running on the operating systems to communicate with each other. …
Resource Management: …
Task Management: …
File Management: …
What are the 10 functions of operating system?
Following are some of important functions of an operating System.
Memory Management.
Processor Management.
Device Management.
File Management.
Control over system performance.
Job accounting.
Error detecting aids.
What are the three main functions of operating system?
What are the functions of the operating system PDF?
Basically, an Operating System has three main responsibilities: (a) Perform basic tasks such as recognizing input from the keyboard, sending output to the display screen, keeping track of files and directories on the disk, and controlling peripheral devices such as disk drives and printers.
What is the function of an operating system Mcq?
Explanation: An Operating System acts as an intermediary between user/user applications/application programs and hardware. It is a program that manages hardware resources. It provides services to application programs.
What is operating system and its functions and types PPT?
An operating system (OS) is a collection of software that manages computer hardware resources and provides common services for computer programs. The operating system is an essential component of the system software in a computer system. Application programs usually require an operating system to function.
What are the functions of operating system class 9?
An operating system is a system software that acts as an interface between the user and hardware resources….Main functions of an OS are as follows:
Storage management.
Does Google Science Fair still exist?
Can you freelance as a journalist?
Who is father of TQM and its history?

redpajama_set_name: RedPajamaCommonCrawl


text:
Who are the Ajaxians? We think of the entire community as Ajaxians, but the folks behind the ajaxian.com site are:
Dion Almaer
Dion Almaer is the director of Developer Relations at Palm where he has the pleasure of working with Ben Galbraith. The pair co-founded Ajaxian.com together and the are now focused on delivering a fantastic developer experience on the mobile Web.
Dion has been a technologist and a developer writing Web applications since it took over from Gopher. He has been fortunate enough to speak around the world, has published many articles, a book, and of course covers life the universe and everything on his blog at almaer.com/blog.
He has been called a human aggregator, and you can see that in full force if you
follow him on Twitter @dalmaer.
Ben Galbraith
Ben Galbraith is the director of developer relations at Palm and the co-founder of Ajaxian.com. Ben has long juggled interests in both business and tech, having written his first computer program at six years old, started his first business at ten, and entered the IT workforce at twelve. He has delivered hundreds of technical presentations world-wide, produced several technical conferences, and co-authored over a half-dozen books. He has enjoyed a variety of business and technical roles throughout his career, including CEO, CIO, CTO, and Chief Software Architect roles in medical, publishing, media, manufacturing, advertising, software and internet industries. He lives in Palo Alto with his wife and five children.
Michael Mahemoff
Michael Mahemoff is a hands-on software developer who previously worked at Google and Osmosoft. He is the creator of the cloud podcast app, Player FM. Building on psychology and software engineering degrees, he completed a PhD on design patterns for usability. He's the founder of AjaxPatterns.org, an Ajax design reference soon to be published as the "Ajax Design Patterns" book, and the creator of the corresponding Ajax Demos. Michael has run conference sessions on agile topics such as Extreme Usability and Self-Documenting Software. Java/J2EE has been the dominant programming platform in his career, though personal projects have used Ruby, PHP, and plain-old Bash. His blog and podcast covers a mix of Ajax, agile, programming, and the occasional usability rant.
Rey Bango
Rey is an industry veteran, with over 19 years of experience in information technology. He brings a unique perspective to RIA development having built true desktop applications for 8 years prior to moving into web programming and being keenly aware of the challenges involved in building desktop-like web applications. Rey is also member of the jQuery JavaScript library's Core Project Team.
He's developed a wealth of knowledge stemming from his work with such technologies as client/server, OOP, PowerBuilder, Sybase, ASP, ColdFusion, DHTML, & Ajax. His blog can be found at reybango.com.
Andrea Giammarchi
Andrea Giammarchi is a full stack web developer with nearly 10 years of hands-on experience working in the field. Starting as server side and database developer, but constantly updated thanks to his passion, Andrea has recieved his ActionScript 2.0 Developer certification in 2004, a year before the ZCE (Zend Certified Engineer) one.
He has been always focused on Web standards, performances, best practices or innovative solutions, deciding at some point to abandon ActionScript in order to dedicate more time over JavaScript, Ajax, and "zero plug-ins" RIA.
Currently employee in London as Engineer for a 100% JavaScript/Ajax desktop like application, Andrea is often trying to contribute for different Web related projects, sometimes inspiring some new technique via his 100% ugly blog: WebReflection
Chris Cornutt
Chris Cornutt is mainly a PHP developer, and has been working with the language for over 6 years now. He also runs the PHP news/community site, PHPDeveloper.org. He has recieved his ZCE (Zend Certified Engineer) and is very involved in the PHP community.
Chris has been published in serveral sources, including a selection from the Worx book "PHP String Handling" and several issues of PHP Magazine on a wide range of topics. He is also a part of the newly formed php|architect's Pro::PHP podcast, developing and recording the podcasts' bi-weekly newscasts.
Salil Deshpande
Salil Deshpande is a Silicon Valley veteran and insider. He advises Ajaxian and finds scoop on Ajax and Web 2.0 happenings in the valley and beyond. Salil is muddling through ideas as Partner at Bay Partners, a venture capital firm, where he also helps find and evaluate investments in Ajax, open source, and online communities. Prior to that he was CEO of several companies, including The Middleware Company, which operated sites such as TheServerSide.com and TheServerSide.NET.
Dietrich Kappe
Dietrich Kappe is a co-founder and the CTO of Pathfinder Associates, LLC, a hybrid User Experience Design and RIA development shop. Dietrich published one of the first 100 public web sites and launched one of the first Java Servlet-based web applications. He has been a software engineer for over 17 years, a frequent open source contributor, and has developed applications for the Media, Financial Services, Insurance and Healthcare industries.
Dietrich is a technical speaker on Agile Software Development, AJAX and Business Rules technology. He publishes the Agile Ajax and Business Rules blogs.
Rob Sanheim
Rob Sanheim is a software developer with over six years development experience and over ten years of IT experience. He is a Sun Certified Java Programmer with extensive experience in developing web applications. Rob has experience in a variety of Java open source frameworks, including Spring, Hibernate, and Struts.
His passions include test-driven development, agile methodologies, and playing around with Ruby to keep his skills up until he can get paid for it. Rob has also done a considerable amount of work with Ajax applications and is a co-editor for Ajaxian.com. He is currently employed with the Madison based consulting firm Smart Solutions. His blog on all things relating to software can be found at robsanheim.com.
Chris Heilmann
Chris Heilmann has been a web developer for over years, after being a newscaster, audio producer and radio journalist for two. He works for
Yahoo in the UK as trainer and web architect and oversees the code quality on the front end for Europe and Asia. Previously he worked for several agencies and dotcoms and created multinational and -lingual sites for clients like HP, McDonalds and VisitBritain.
He is very much dedicated to creating a usable, accessible and future-proof web and is agnostic to the technologies involved to build them – as long as they produce code that adheres to an understandable standard. He is a strong believer in a move from web development as a technical problem to seeing it as a matter of teamwork and different layers of technology and skillset working seamlessly together.
He's published several books on the topics of accessibility, JavaScript and creating web products using APIs and hosted services.
He blogs at http://wait-till-i.com and is available on many a social
network as "codepo8.".
Brad Neuberg
Brad Neuberg is a developer advocate at Google for the Open Web, focused on HTML 5, SVG, and more. He is the creator of a number of JavaScript libraries and frameworks for expanding the capabilities of web applications, including Dojo Storage, Dojo Offline, and Really Simple History. Brad worked with Douglas Engelbart on the HyperScope project; explored deeply collaborative web browsers with Paper Airplane; worked on one of the first web-based RSS aggregators; and was a Developer Advocate for the Gears project. He is currently working on the SVG Web library, a drop-in JavaScript toolkit that brings SVG 1.1 support to Internet Explorer. Brad also created Coworking, an international grassroots movement to establish a new kind of workspace for the self-employed.
Brad blogs at Coding in Paradise and Twitters at bradneuberg.
José Jeria
I am a self-taught developer that started doing web development back in 97 in Stockholm Sweden. I worked in different web agencies and ended up in Munich Germany after joining an American company called Razorfish. I worked as a web developer mainly coding HTML / CSS and JavaScript etc for 8 years before I got into developing back-end in Java (J2EE) as well.
The most fun I have though, is when developing rich front-ends though (I am very keen on user interface design). I have been, for the last 5 years, developing intranet web applications in data-warehouse environments using different frameworks, such as JSF, Spring MVC and lately my new favorite: Ext-GWT.
Check out Ajaxian.com's sister sites:
TheServerSide.com is the largest independent Java community in the world, providing daily news, tech talk interviews with key industry figures, design patterns, discussion forums, tutorials, and more.
SearchSoftwareQuality.com provides the most relevant information on software quality management, software requirements, testing, QA, security, project management, development models, and more.
SearchWinDevelopment.com is a unique online resource for developers, architects and development managers tasked with building and maintaining enterprise applications using Visual Basic, C# and the Microsoft .NET platform.
SearchSOA.com is the most relevant and extensive online community dedicated to service-oriented architecture (SOA).
ebizQ.net is the definitive venue for business and IT professionals, vendors, and industry analysts with the need to exchange information on enterprise technologies, problems, and solutions. ebizQ focuses on business enablement, including SOA, BPM, integration, Business Intelligence, SaaS, and security.
About TechTarget
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For inquiries about Ajaxian.com, contact TechTarget at 617-431-9200.


text:
Mariner 4 studies Martian surface
The unmanned spacecraft Mariner 4 passes over Mars at an altitude of 6,000 feet and sends back to Earth the first close-up images of the red planet.
Launched in November 1964, Mariner 4 carried a television camera and six other science instruments to study Mars and interplanetary space within the solar system. Reaching Mars on July 14, 1965, the spacecraft began sending back television images of the planet just after midnight on July 15. The pictures–nearly 22 in all–revealed a vast, barren wasteland of craters and rust-colored sand, dismissing 19th-century suspicions that an advanced civilization might exist on the planet. The canals that American astronomer Percival Lowell spied with his telescope in 1890 proved to be an optical illusion, but ancient natural waterways of some kind did seem to be evident in some regions of the planet.
Once past Mars, Mariner 4 journeyed on to the far side of the sun before returning to the vicinity of Earth in 1967. Nearly out of power by then, communication with the spacecraft was terminated in December 1967.
https://www.history.com/this-day-in-history/mariner-4-studies-martian-surface
MarsSpace
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Pike expedition sets out across the American Southwest
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Fashion designer Gianni Versace murdered by Andrew Cunanan in killing spree
Spree killer Andrew Cunanan murders world-renowned Italian fashion designer Gianni Versace on the steps outside his Miami mansion. Versace is shot twice in the head, and Cunanan flees the scene. Cunanan had no criminal record before the spring of 1997, when he began a killing ...read more
Nixon announces visit to communist China
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Second Battle of the Marne begins with final German offensive
On this day in 1918, near the Marne River in the Champagne region of France, the Germans begin what would be their final offensive push of World War I. Dubbed the Second Battle of the Marne, the conflict ended several days later in a major victory for the Allies. The German ...read more
Senator Barry Goldwater nominated for president
Senator Barry Goldwater (R-Arizona) is nominated by the Republican Party to run for president. During the subsequent campaign, Goldwater said that he thought the United States should do whatever was necessary to win in Vietnam. At one point, he talked about the possibility of ...read more
Jimmy Carter speaks about a national "crisis in confidence"
On this day in 1979, President Jimmy Carter addresses the nation via live television to discuss the nation's energy crisis and accompanying recession. Carter prefaced his talk about energy policy with an explanation of why he believed the American economy remained in crisis. He ...read more
Columbia Records drops country legend Johnny Cash after 26 years
The critically acclaimed 2002 biopic Walk The Line depicts the life and career of Johnny Cash from his initial rise to stardom in the 1950s to his resurgence following a drug-fueled decline in the 1960s. The selection of this time span made perfect sense from a Hollywood ...read more
"Die Hard" debuts, makes Bruce Willis a movie star
On this day in 1988, Die Hard, an action film starring Bruce Willis as wisecracking New York City cop John McClane, opens in theaters across the United States. A huge box-office hit, the film established Willis as a movie star and spawned three sequels. Die Hard also became ...read more
A notorious English killer is executed
John Christie, one of England's most notorious killers, is executed. Four months earlier, on March 25, the police and a tenant at 10 Rillington Place in West London made an awful discovery: the bodies of four women in an empty apartment, three in a hidden cupboard and one more ...read more
Ford Motor Company takes its first order
On this day in 1903, the newly formed Ford Motor Company takes its first order from Chicago dentist Ernst Pfenning: an $850 two-cylinder Model A automobile with a tonneau (or backseat). The car, produced at Ford's plant on Mack Street (now Mack Avenue) in Detroit, was delivered ...read more
Lafayette selected colonel-general of the National Guard of Paris
On this day in 1789, only one day after the fall of the Bastille marked the beginning of a new revolutionary regime in France, the French aristocrat and hero of the American War for Independence, Marie-Joseph Paul Roch Yves Gilbert du Motier, Marquis de Lafayette, becomes the ...read more


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Q: Enable Datepicker only when first field has a value Right now, the End Date selection is disabled. I want to only enable this when a Start Date is selected.
if( $('#datepicker1').val().length === 0) {
    $('#datepicker2').datepicker("disable");
} else {
    $('#datepicker2').datepicker("enable");
}

This clearly does not work. If I insert value = 'random date' into my first input field, it works fine. I'm not too sure on how do this. Clearly not as easy as I had hoped.
My other problem, or hope, is to disable the dates including and before the first selection.
You know, pick Start Date, and every date before and said date for the next picker would be disabled. But that is a whole other problem.

A: I would use the getDate method and see if it's null (nothing selected/entered), like this:
if($('#datepicker1').datepicker("getDate") === null)

For the other issue, check out the date range demo for the datepicker, it has a start/end date like you're aiming for.

A: Just try this approach -
$('#datepicker1').datepicker({

     //your other configurations.

     onSelect: function(){

    //enable datepicker 2 over here.

    }
 });

A: You can use something like this:
var end = $('#end').datepicker();

// Defining a function, because we're binding this to two different events
function enableEnd() {
    end.attr('disabled', !this.value.length) // Enable the end input element if the first one has anything in it
       .datepicker('option', 'minDate', this.value); // Set the minimum date to the date in the first input
}

$('#start').datepicker({
    onSelect: enableEnd // Call enableEnd when a date is selected in the first datepicker
}).bind('input', enableEnd); // Do the same when something is inputted by the user

It's not really a good idea to enable the datepicker in the second field only after the first has been filled in, because the user can still add things into the second field manually, and you lose the format validation usually offered by jQuery UI datepicker. Instead, we disable the second input element directly.
See it working here: http://www.jsfiddle.net/yijiang/KwhLw/
Also note that we're using the input event here, because although it has less broad compatibility, is better than the usual methods used for keyboard event capturing. See a full discussion on this here: http://whattheheadsaid.com/tag/oninput

A: Well, question is answered. For those who want to know what I have, here it is.
To change a Start Date and an End Date (A date range if you will) into an array of individual dates, I used this:
function createDateRangeArray($strDateFrom,$strDateTo) //Changes a Range of Dates to Specific Dates
    {
    static $aryRange = array(); //Creates an Array

    $iDateFrom = mktime(1,0,0,substr($strDateFrom,5,2),     substr($strDateFrom,8,2),substr($strDateFrom,0,4));
    $iDateTo = mktime(1,0,0,substr($strDateTo,5,2),     substr($strDateTo,8,2),substr($strDateTo,0,4));

    if ($iDateTo >= $iDateFrom)
        {
        array_push($aryRange,date('Y-m-d',$iDateFrom)); // first entry

        while ($iDateFrom<$iDateTo)
            {
          $iDateFrom += 86400; // add 24 hours
          array_push($aryRange,date('Y-m-d',$iDateFrom));
            }
        }

    return $aryRange; //Returns to step 1 and adds another value into the array
    }

To get every date from my SQL Database and push them into a single array, this was used:
$query = "SELECT startdate, enddate FROM classdetails";
$results = mysql_query($query);

while ($arrays = mysql_fetch_array($results))
    {
    $aryDates = createDateRangeArray($arrays['startdate'],$arrays['enddate']);
    echo "
";
    }

So now I have managed to get every date range from an entire list of classes and made one huge array.
Now I had to use this array to actually disable the dates. Using the functions of which Yi Jiang has no generously wrote (thank you to everyone who helped me), the next step is:
$(function()
            {
            //To enable End Date picker only when Start Date has been chosen (And to disable all dates prior of said date)
            var end = $('#enddate').datepicker( {numberOfMonths: 3, beforeShowDay: checkAvailability,});

            // Defining a function, because we're binding this to two different events
            function enableEnd() {
                end.attr('disabled', !this.value.length) // Enable the end input element if the first one has anything in it
                   .datepicker('option', 'minDate', this.value); // Set the minimum date to the date in the first input
            }
            //End of function

            // Datepicker
            $('#startdate').datepicker({
                numberOfMonths: 3,
                beforeShowDay: checkAvailability,
                onSelect: enableEnd // Call enableEnd when a date is selected in the first datepicker
            }).bind('input', enableEnd); // Do the same when something is inputted by the user

            //hover states on the static widgets
            $('#dialog_link, ul#icons li').hover(
                function() {$(this).toggleClass('ui-state-hover');}
            );
            });
        //End of Function

        //Disabling all dates where selected room and speaker is unavailable
        var $myBadDates = new Array (<?php foreach($aryDates as $disabledate) { echo " \"$disabledate\","; } echo " 1"; ?>); //Creates the array (The echo " 1"; is merely to close the array and will not affect the outcome

        function checkAvailability(mydate){
        var $return=true;
        var $returnclass ="available";
        $checkdate = $.datepicker.formatDate('yy-mm-dd', mydate);
        for(var i = 0; i < $myBadDates.length; i++)
            {
               if($myBadDates[i] == $checkdate)
                  {
                $return = false;
                $returnclass= "unavailable";
                }
            }
        return [$return,$returnclass];
        }
        //End of function

The only thing in my body right now, for testing purposes, are:

Datepicker

    Start Date: <input type="text" id="startdate" />

    End Date: <input type="text" id="enddate" disabled="disabled" />

It's long, yes, but it works. Thank you to everyone who helped me get this working.
The edit was me changing a function to a JQuery function that exists (of which for some reason I did not use in the first place); toggleClass. Thanks for picking that out.

redpajama_set_name: RedPajamaStackExchange


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TiVo has expanded the content options available on the Bolt, TiVo's new 4K-capable DVR platform, with access to two over-the-top subscription video services – Hulu and WWE Network.
Among the new batch, Hulu now sells its traditional subscription-advertising hybrid as well as a new ad-free option, while WWE Network runs $9.99 per month.
TiVo introduced the Bolt in October. The new four-tuner device, which starts at $299.99, supports 4K streaming, pay-TV services (via the CableCARD), and a new "Skip Mode" feature that lets users skip commercial breaks in recorded shows on nearly two dozen channels, including the major broadcast networks. TiVo initially developed Bolt as a retail product, but is expected to offer a version that is tailored for TiVo's MVPD partners.


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Q: How to get value of 'this' inputbox? I am writing a web application where the user clicks on a div, that is holding a input text box with predefined text in it. When the user clicks on the div the code is then printed in a separate text box. I am trying to write a function that grabs the value of the the clicked on div's text input. I have it working by clicking on the input box itself by using     $(this).val(); but I want to click on the div and then it essentially gets the value of (this)('input[type=text].provided_code').val();
is there a way to say the text input inside this div? There are like 20 div's on the page with 20 inputs in each div, and each have the same class name etc.

A: Yes, you can do:
$(this).find("input[type='text']").val();

Assuming that there is one input of type text inside that div.

A: Yes you can specify the selector context:

By default, selectors perform their searches within the DOM starting at the document root. However, an alternate context can be given for the search by using the optional second parameter to the $() function

Documentation:
http://api.jquery.com/jQuery/#jQuery1
So you code could look like this:
$('input[type=text].provided_code', this).val()

Performance:
http://jsperf.com/jquery-find-vs-context-sel/38

A: Instead of (this)('input[type=text].provided_code').val();
you should use a correct jQuery with the find function.
$(this).find('input[type="text"].provided_code'].val();

A: You can use find - Although, you cannot target a specific input on click of your div unless that input has a unique class or id.
$('div').on('click',function(){
  var value = $(this).find('input[type=text].provided_code').val();
})


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Home » News » COVID-19 news » Give estate agents more clarity on what is essential work, pleads leading industry figure
Give estate agents more clarity on what is essential work, pleads leading industry figure
Ed Mead says the industry needs better advice and that the furlough scheme will have to be re-evaluated as the UK comes out of the crisis.
9th April 2020	2 Comments 4,396 Views
Senior industry figure Ed Mead has called for the government to give the industry more clarity on what is 'essential work'.
He has also predicted that ministers will have to look at the furlough scheme as the crisis begins to ease in order to allow estate agencies and other businesses to plan how they are going to return to normal trading conditions.
This would include allowing furloughed staff to being working again but still receive some or all of their monthly government payments, and allow agencies to ease back to normality.
Mead says he temporarily suspended operations at his outsourced viewings company, Viewber, which uses the services of several thousand self-employed operatives around the UK, once the lock-down was announced, but would love to utilise them.
But he says Viewber can't because Ministry of Housing guidance has yet to be issued that is crystal clear about the work of estate agents and what is 'essential'.
Currently, the advice is that: "Employers should take every possible step to facilitate their employees working from home. Where it is not be possible to work from home you can still travel for work purposes, provided you are not showing coronavirus symptoms and neither you nor any of your household are self-isolating".
Asked what he thinks negotiators and valuers should be doing now, Mead says his experience, gained through several tough times including the 2008 financial crisis, is that no one remember what you did to them during a downturn, but "they always remember the feeling".
"So in a disaster like this agents should be contacting customers to make them understand how sorry they are about what's happening," he says.
"It's more important to find out how they are feeling, rather than just trying to transact – treat them like human beings."
Watch the interview in full.
furlough scheme Ed Mead Viewber	April 9, 2020
9th April 2020 at 9:17 am
You are a long time dead, having experienced the deaths of six estate agents in the past week all of whom I know personally, anything that keeps people alive is in my view a good policy.
Sweden is going for a different approach, and in parts of America, Realtors are considered to be essential or key workers, but movement of people is in my mind likely to result in more fatalities than reduce them.
Money commerce and the ability to provide is essential, but not as essential as being able to wake up in the morning alive.
Yes social distancing can be operated, but each time an agent gets into a car and goes to get petrol, get a sandwich, they are potentially endangering themselves and others. If you add a multiplier to this, soon you see why the number of people sadly infected and dying increases.
Philip Michael Priest, 4Corners Property Ltd 4Corners Property Ltd
Andrew I completely agree.
If they carried out the viewing and agreed the sale, firstly nothing will complete until September at the earliest. This due to valuations not being carried out, lending pretty much on-hold and most banks working on skeleton staff, solicitors working on similar measures, but then other services like removals not being available either.
Just one other point, if you agreed the sale this week, caught corona-virus, passed it on to the others buying the house, then what good is the new home or the commission when you are no longer on this planet to enjoy it??
The only part of the property business in operation should be inspections which can be done via video link with the tenant (and record if you know how) and emergency call outs.
Stay at home, protect yourself, save YOUR life!


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Chipotle Is Launching a New Line of Organic Lemonades, Agua Frescas and Iced Tea
Sip on a refreshing beverage while giving back to farmers.
Credit: Getty Images / SOPA Images / Contributor
Chipotle is known for their customizable menu, which makes it easy to order a healthy and filling meal. The company is constantly rolling out new menu items, like their most recent addition of cauliflower rice, and their latest drink offerings sound like the perfect way to cool off this summer.
Related: How to Order Healthy at Chipotle
According to a media release, Chipotle will sell five different beverages from Tractor Beverage Co., a company that makes certified organic, non-GMO products, starting on July 21. If you're dining in the restaurant or getting takeout, you can choose from drinks like lemonade, hibiscus lemonade, mandarin agua fresca or berry agua fresca. And if you're opting for delivery, you can choose from bottled lemonade or black tea, plus the four drinks available in-store.
These new beverages sound like the perfect side for any burrito bowl or quesadilla. And as an added bonus, 5% of profits from the sales of these beverages will go towards Chipotle's programs that help to protect the future of farming.
So the next time you're placing an order at Chipotle, consider trying one of these delicious beverages on the side. Not only will you have a fruity and refreshing drink to help you stay hydrated in the summer heat, but you'll also be giving back at the same time.
Related: Almost Chipotle's Guacamole


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Tag Archives: Butter
Beijing Sanyuan Foods and Fosun Close to Purchasing France's St Hubert
Jul 29, 2017 Dairy (Milk)Acquisition, Beijing, Butter, France
Fosun International, the Chinese insurance-to-tourism conglomerate, and Beijing Sanyuan Foods are close to a joint deal to buy French margarine and health food maker St Hubert from Montagu Private Equity, according to a joint statement from the two Chinese firms…Full Article: South China Morning Post July 2017 Key Points The Chinese acquisition of St Hubert,
Beijing Sanyuan Foods, Sole Survivor of the 2008 Melamine Scandal, To Purchase Canadian Dairy Company
Jul 18, 2016 Dairy (Milk)Acquisition, Beijing, Butter, Canada, Cheese, Dairy, Ice Cream, Yogurt
Beijing Sanyuan Foods Co Ltd, one of China's leading dairy producers, plans to purchase a majority ownership in Crowley Properties Ltd, a Vancouver-based company making dairy products such as yogurt, cheese, ice cream and butter for about C$19 million ($14.58 million), according to an announcement by Sanyuan. The acquisition was approved by Sanyuan's board of
New Zealander Exports to China Fall On the Back of Declining Milk Powder Prices
Feb 27, 2015 Dairy (Milk)Butter, Cheese, Dairy, Milk Powder, New Zealand, Prices
New Zealand exports to China last month were less than half the value of January 2014, leading a fall in the country's total goods exports, the government statistics agency announced on Thursday [26 February 2015]. Total exports were down by 9.1 percent year on year to 3.7 billion NZ dollars ($2.79 billion) in January, according


In their annual wellness trends collection, W+G claims MCT Oil is going mass market, and quotes NOW® Sports Brand Manager, Bryan, as an industry-leading authority.
Kelly LeVeque shared her post-baby self-care tips, including bathing with NOW's Magnesium Flakes, taking her daily supplements and of course, making her Fab Four Smoothie.
NOW DHA-500 is recommended as a supplement to support brain health.
In an article about snacking like a personal trainer, #NOWWellness Influencer, Kasey (@powercakes), recommended NOW® Sports Eggwhite Protein to whip up overnight oats and smoothies.
A great endcap to our 50th Anniversary, Taste for Life features NOW as pioneers of the natural product industry.
MindBodyGreen's wellness editor, Gretchen, touts NOW® Solutions Hyaluronic Acid Serum as one skincare product she can't live without.
NOW® Elderberry and NOW® Allibiotic were among 13 supplements featured to support immunity, as recommended by NOW wellness partner Dawn Jackson Blatner and #NOWWellness Influencer Chrissy Carroll.
Kelly LeVeque shared her morning routine with ABC/GMA digital, including our #BodyLoveNOW50 smoothie builder.


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Samsung 2021 TV's have Mini LEDs Built-in
Samsung is releasing Neo QLED 8K (QN900A) and 4K (QN90A) sets are set to use mini LEDs, and apparently the 12-bit, 4,096-step luminance won't compete with OLED's "perfect" contrast ratios, but it should make bright colours brighter and darker colours darker than regular LCDs. Samsung says the LEDs in these TVs are up to 40 […]
TikTok comes to your Samsung TV in the UK and Europe
As many of you know, TikTok is spreading like wildfire, with over 500 Million active monthly users. Now, Samsung and TikTok have announced an exclusive deal that will see the App come to Samsung Smart TVs. Availability will be in 39 languages spread over 150 markets. Obviously the app will tailored for the "home-viewing experience". […]
Samsung Tizen OS is now the Largest TV Platform
According to the latest numbers, the Tizen OS is the largest TV streaming platform in the world. The OS has been developed by Samsung which is then used in smart TVs and smartwatches. The research conducted by the market research company, Strategy Analytics, has said that Samsung had sold 11.8 million TVs worldwide during Q3 […]
Google Assistant is now rolling out to 2020 Samsung Smart TVs
Samsung has announced that it will be bringing Google Assistant to its latest 2020 Smart TV's. Initially, the rollout will take place in France, Germany, Italy, and the UK. Phase two of the rollout will target Brazil, India, South Korea, and Spain. Samsung has also mentioned that a further 6 countries by the end of […]
Samsung TV Plus is Now Receiving Three New Channels!
Samsung TV Plus has now got three new channels from Endemol Shine. The Endemol Shine Group is a British-Dutch production and distribution company. They have announced that they're bringing three channels to Samsung TV Plus. Two of these channels are going to Samsung's video streaming service in the US. These channels are called Deal or […]
Samsung TV Plus Streaming Service Could Come To Mobile!
Samsung plans to bring its TV Plus free streaming service to its mobile devices. The mobile app is currently in the development stage in order to deliver the same functionality that is available on compatible Smart TVs. TV Plus was first introduced last year as Samsung's free streaming service and is available in the companies […]
The Google-Amazon Tech Feud Spilling into Smart TVs
We all know about the grudge that Google has against Amazon. Both of the companies were kicking each other off of their own platforms. For example, Google revoked YouTube from being available on Amazon's Fire TV platforms. Google make manufacturers agree to terms and conditions Now we are at the stage where the tech giant […]
Netflix will Drop Support for Some Samsung TVs this year!
That's right people, starting on December 1st this year, Netflix is not going to support the older Samsung smart TVs. Netflix is sending out error messages to the TVs of the affected people. Whilst they are doing that, Samsung have written about the news on their official webpage. On Samsung's post about this event, they […]
Regularly scan your Samsung Smart TV for Viruses
Recently on Samsung's "Samsung Support USA" Twitter account, they had posted a small 19-second video. On what? On how to check your Samsung smart TV for viruses or "malicious software attacks". They also said that users should do this regularly. When asked if this tweet was prompted with any threats, the company said that they […]
LG announces the sales of their first 8K OLED TV
On the 3rd of June, LG Electronics announced the start of their first 8K OLED TV. The pre-orders for this 88-inch TV start in South-Korea this week but will come to the key markets (America and Europe) in the third quarter of the year. 8K TV increases viewer immersion with improved audio performance, largely due […]
Samsung Smart TVs start getting Apple TV app and AirPlay 2 in Europe
Apple TV and AirPlay 2 support has finally arrived on Samsung Smart TVs. Compatible Samsung TVs, which include all 2019 and select 2018 smart TV models, are receiving a firmware update which brings the two new apps. Samsung had announced the support for Apple TV and AirPlay 2 during the Consumer Electronics Show 2019 in January. Earlier […]
2019 LG TVs will soon get Alexa, Airplay 2 and Apple HomeKit support
After adding Google Assistant on its 2018 TVs, LG is now introducing Amazon Alexa to its 2019 TVs with ThinQ AI. Starting this month, LG's 2019 lineup of Smart TVs featuring ThinQ AI, including UHD TVs, NanoCell TVs and OLED TVs, will get support for Alexa voice assistant. The support will be rolled out through […]
Apple TV and AirPlay 2 support rolling out for Samsung Smart TVs
Samsung had announced support for iTunes and AirPlay 2 on its Smart TVs during the Consumer Electronics Show 2019 in January. The company has now begun rolling out the Apple TV app and AirPlay 2 support to all of its 2019 Smart TVs and select 2018 TV models. The new Apple TV app will be […]
Hulu lowers the price of its most popular plan, now at $5.99 per month
Popular video streaming service Hulu has announced plans to drop the price of its most popular plan. Starting next month, the ad-supported $7.99 plan will drop to $5.99 per month. The price includes all of Hulu's on-demand programming from participating channel providers, as well as Hulu's slate of original content. The streaming market is getting […]
LG smart TVs running webOS can now be rooted
Our "smart life" tech can be a bit restrictive at times. If you want to get a bit more out of it you can sometimes find a way to "root" or "jailbreak". Usually when talking about these things we tend to refer to smartphones, tablets, or even a set-top box. Well, now you can root […]
Samsung are considering ending Tizen TV production in India
Samsung makes many of their products in India, for example, TVs are one of their biggest investments. Now, a report suggests that Samsung are looking to stop the production of TVs in India in favor of imports. It is said that the company are working out plans to import their TV lines from Vietnam instead […]
Samsungs Q900FN QLED 8K TV Unveiled at IFA 2018
During the Samsung press conference at IFA 2018, the company announced their new Q900FN QLED 8K TV. The Smart TV should be available in the United States by October. According to Samsung, the Q900FN will feature all the benefits of Samsung's flagship QLED line. The Q900FN features real 8K resolution and is able to reach a […]
Hulu Live TV now available on LG and Samsung Smart TVs
American subscription video on demand service, Hulu, is a great platform to keep up on your favorite shows, and still have access to an expansive library of on-demand content. And starting today, Hulu is available with Live TV on even more devices across platforms, including LG and Samsung. Platforms that already had Hulu support, like Roku, are getting […]
Samsung to launch Samsung Music app on Smart TVs
Samsung Electronics has announced that the Samsung Music app, available on Samsung Galaxy smartphones, will now be available its Smart TVs too. The app will start surfacing on Samsung Smart TVs by the end of April 2018, the South Korean tech giant said. Samsung Music app for Smart TVs Samsung will launch the Samsung […]
Samsung invests $4.6 million on Audioburst, will add its services into Smart TVs
Samsung Electronics have announced a partnership with Audioburst, the revolutionary AI-powered audio search platform, to deliver an incredible new listening experience for consumers. As per the terms of agreement, Samsung will incorporate the Audioburst services into its products globally, starting with Smart TVs. "Audioburst's mission is to organize the world's audio content and now, together with Samsung, we […]


Leading writers, academics and experts are coming to Compton Verney from June 19 to 21 for a festival designed to make people think.
The Also festival promises to help visitors discover how to live better through its philosophy breakfasts, understand the way they eat and connect more fully with nature.
The event welcomes Chocolat author Joanne Harris , offers the chance for everyone to sing at its Rockaoke session and enjoy our closing party with superstar DJ Greg Wilson.
Supervised wild swimming takes place twice a day, while food will be served by the likes of The Black Cab Coffee Co and Vogue's favourite discovery Nina, with a Great Indian Food Feast on the Saturday night.
The children can go on a bat walk and learn to DJ, dance bhangra, hoopercise or even how to knit an egg cosy in one of the many special workshops.
Also is the annual festival run by Salon London, the 'interactive cultural event' that showcases specialists from the world of science, arts and psychology, voted by GQ magazine as number 6 in the Best Things to do in the World in 2014.
Weekend tickets start at £75 and cost £170 for a family of four (including camping). There are a limited number of luxury bell tents in its Hotel Safari for £320. Day tickets are also available at £35.


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Athens Municipality Looking for Buildings in the City to Paint Murals On
Tag: art, Athens, Athens mural, contemporary art, culture, Kostas Bakoyannis, l75l, street artists
The Municipality of Athens is searching for buildings to paint murals on aiming to liven up the city center and promote contemporary art in an urban environment.
In the context of its public murals project, after refreshing the city's school buildings with street art, the municipality is extending its program to private buildings located in the center and neighborhoods of Athens.
"Our program is extending to all seven municipal districts of Athens' neighborhoods. Our aim is for the city to become more colorful and for its buildings to become a 'canvas' of contemporary art through the eyes of its young talented street artists," Athens Mayor Kostas Bakoyannis said.
The city center's residents, organizations, public and private bodies can contact the municipal services of Athens and propose their own wall surfaces that could be used for the development of murals, provided that their properties are within the municipality's limits.
Those interested can send their property's address, a photo of the wall's surface and their contact details via e-mail to cityhallculture@cityofathens.gr.
Athens' latest murals were recently created on the walls of the 104th Elementary School and the 18th Lyceum (high school) and are dedicated to Greek painter Theofilos and poet Andreas Kalvos.
According to the municipality, two more school buildings will unveil their murals by the end of the year.
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Mr. Anonymous 18 November 2021 at 11:17 Reply
Athens does not only belong to the rich and famous. Share the wealth and bring murals and vibrancy to the hard working middle, lower class and immigrants. There are plenty of building in these areas with large empty faces that could be used. They are people also that work hard and pay taxes for you!!!
GTP editing team 18 November 2021 at 11:30 Reply
If the buildings you are referring to are in one of the seven municipal districts of Athens, they are eligible to be included in the initiative.
Good decision and move. Now let's see if their promises will be kept. Please focus on the poor and immigrant sections of Athens that desparately needed to be brightened and promoted. I am waiting!!!


front and back. So I decided to start to paint F & B first, rather than last. It is a work in progress. So go across to the stamping ground and take part and show your desks.
I have used Paperartsy Fresco paints, Decoart moulding paste for textureand some embossed paaper.
This is the view from my workroom, Its a terrace, my Delilah is taking advantage of the first full suuny day we have had in ages. this was yesterday.
another view of my garden from the terrace, nice and lush due to all our rain..
OOOOOOOOH love your garden!!!!!! My kind of space.
Like the treatment you're giving the journal. Nice to see you re experimenting with textures.
love the colour of your journal, my favourite, your garden looks very peaceful, make the most of the sun.
Wow the colours on here are stunning. Really show the texture. love it.
Fabulous bit of texture on your covers and your garden is looking good too.
Such a pretty journal page! Love the texture!
What a gorgeous view from your desk! And your journal looks fascinating! Great texture! Happy WOYWW and thanks for visiting my area!
Love your book and sunbathing kitty!
Love your journal cover pages. I've never had a go at anything like that yet, I might have to give it a go.
that journal looks beautiful! the texture is lovely! your view is also so beautiful. so glad to stop by today.
Gorgeous journal cover, Francesca - the colour and texture is great. Nice to see a kitty enjoying the small amount of sunshine we've had!
Thanks for your comment - yes, you certainly need the pink one as it's really juicy! Have you got the purple one? They are great together.
Love your garden!! That's a very nice space indeed - your cat certainly seems to be admiring it :) Love the bright colours of the journal - not for shy retiring wall flowers, I think!!
So glad i could catch up with you again this week. Is that sun I see in your garden??!!! You lucky thing. What a fab outlook. I have had some dylusions Inks in the post this morning and can't wait to try them, but I love the texture youve got from the paste. Might try it with the inks I've got.
Wow! What a pretty lush garden and kitty has the right idea, to soak up the sun. The journal cover is looking good. I like the texture to it, that really adds to it. Thanks for the WOYWW visit. Hope you're having a good day.


There are type-A personalities and then there is Jen. She brings a whole new level to the term hard working it doesn't matter if we asked her to run as fast as she could or to do 225 push-ups she just did it. Every once in a while with a little statement of doubt, but always did it.Jen came to us looking to increase her lean body mass, she already had a low body fat, we just needed to bring her muscle mass up. Now we don't really have a way of measuring her other goal of being more confident, but looking at her pictures I'd be troubled to say this wasn't a confident person, a good rule of thumb is that if you're standing in your underwear in front of a camera you must be confident about something.Through Jen's hard work she hit her goals, we were able to make her muscles "pop" and get some awesome shots.
Something you wouldn't expect from someone who is so lean is that she is an awesome baker. And she treated us to some of those delicious treats. Jen's baking was great but wasn't the most memorable thing about her shoot. Never before had someone brought a "script" of what she wanted to shoot. When she got there she found the biggest table and rolled out her master plan. It made our life super easy, just follow the script.
Jen you did awesome during your time here with us, very proud of you! Keep tackling everything you do with that all-or-none attitude!


Come together on the first day of the expo before the ribbon is cut when Morten Hansen, one of the leading management authorities of our time, will set the stage for this year's United Fresh Convention & Expo as keynote speaker during the United Fresh Breakfast General Session. United Fresh's Produce Industry Leadership Class 24 also will be graduating Tuesday morning. Share what's motivating them to drive our industry forward!
All attendees at the general session will receive a copy of Hansen's bestseller, Great at Work.
Morten Hansen's Wall Street Journal bestseller Great at Work is based on his exhaustive study of 5,000 employees, showing how top performers do less, work better and achieve more.
Hansen also is the co-author with Jim Collins of the bestseller Great by Choice on how businesses can thrive in uncertainty. He also is the author of the acclaimed book Collaboration describing how managers can overcome silos in a company and create real value from working across the organization.
As a leading authority on business management, we're excited to hear how Morten Hansen would advise OUR industry based on his experience. Submit your pressing business management question and we'll share them with Hansen as he prepares to address our industry.