We have sought to provide a six-month plan of events covering all aspects of Old Suttonian engagement, whether that be social events, School events or sporting fixtures. We hope that this advanced planning will maximise the number of Old Suttonians who are able to attend the range of events on offer. The upcoming Old Suttonian events are listed below.
This year will see the fifth annual Old Suttonians' Golf Day. The event, at The Ridge Golf Course, will feature a singles competition and a team competition. Whether you are coming alone, with a friend or as a team of four, you are most welcome to take part. For those not able to register as a team, individuals will be matched to make a balanced four with Stableford rules applying.
The day will start with bacon rolls, tea and coffee from 11.45am. The golf will then begin at 12.30pm and the day will end with an evening meal and small prize-giving ceremony. Given the School's connections to The Ridge, which is owned by an Old Suttonian, we are able to offer this year's Golf Day at the rate of £40.00 per person. Please book using the OS Golf Day page. If you would like further information, please contact David Pickard (Staff 1977-2001, 2009-2015).
This year, the annual Sergison Trophy will take place on the early May Bank Holiday weekend. This is a .22, four-way shoot which is team dependent - School team, parent team, staff team and an Old Suttonian team. The competition is due to start at 11.00am. As usual, lunch will be provided in the form of a barbecue at the back of the range.
We hope to have a strong OS team competing, so please do come along – all equipment will be supplied and training will be given. If you would like to take part, or would like to come along to watch, please email Glen Millbery (Staff 2000-). If you would like to register a group, please provide Glen with the requisite details for all competitors. If you would like further information about OS Shooting in general, including information on the newly formed Old Suttonians Rifle Association, please refer to the OS Shooting Page.
Old Suttonians are invited to attend the School's Summer Music Concert on 8th May. The event was hugely over subscribed last year, so it has been moved to the All Saints Church, Maidstone to accommodate a larger audience. We hope you will be able to join us for an evening featuring the Chapel Choir, Chamber Choir and The Strings playing a range of pieces from the likes of Handel, Parry, Mendelssohn and Rachmaninov.
It is always a fantastic programme which, in part, serves as a farewell to our Upper Sixth musicians. This year, we will also be saying farewell to our Assistant Director of Music, Jonathan Soman (Staff 2013-2019), ahead of his move to the RGS Worcester, so it will be a chance for the School community to say goodbye. There is no need to pre-book tickets but we would ask that you please email the Development Office to indicate your intention to be there.
Last year, the School hosted the inaugural Cope Cup fixture, a three-team Tennis tournament contested between pupils, staff and parents. Following the success of that event, the decision has been taken to expand the competition to a four-team format, allowing Old Suttonian Tennis players to compete. The competition, starting at 2.30pm is open to all OS and we are hoping to field as team of at least four players.
After the matches, there will be a barbecue at TCs, which will hopefully be an opportunity for Old Suttonians to chat to one another and with others from the broader School community. If you would like to take part, please contact the Development Office for more information.
With the SVS Car Show due to return next year, the focus this year is entirely on the Cricket with an Old Suttonian XI taking on the School's 1st XI. Unfortunately, last year's match had to be cancelled due to the weather, so we will be hoping for better conditions this year. The match is due to start at 11.30am on The Upper.
If you would like to play in the match, please contact the OS match manager – Chris Vernon. Alternatively If you would simply like to come along and watch, we look forward to seeing you there, no pre-registration is required. For more information about Old Suttonian Cricket in general, please refer to the OS Cricket page.


text:
\section{Introduction}

It is well established that clusters at $z < 1$ are dominated by galaxies with redder colors, older stellar populations, early type morphologies, and little star formation, as opposed to the field environments. Many scenarios related to cluster environments have been proposed to explain how the star formation is ceased in clusters, including processes, such as ram-pressure stripping \citep{gun72,dre83}, and galaxy-galaxy interaction \citep{mih94} that quench star formation over a short timescale, and `strangulation', referring to the removal of warm and hot gas \citep{lar80,bal00}, which slowly reduces the cold gas supply. Studying the quenching timescale for cluster galaxies hence provides a powerful way to constrain the physical mechanisms responsible for the star formation quenching.

One of the tools to constrain the quenching timescale is the comparison of the properties of star-forming galaxies between different environments. It is found that star-forming galaxies (hereafter, SF population) form a tight sequence on the SFR and stellar mass plane, the so-called `main sequence' \citep{bri04,noe07,elb07,dad07,pan09,mag10,lin12,whi12,hei14}. It is expected that slow quenching would lead to an overall reduction of the specific star formation rates (sSFRs) of the SF population whereas a fast quenching mainly changes the fraction of quenched population without altering the sSFR of the remaining SF galaxies.
Previous studies have suggested that the difference in the star formation activities between the field and the cluster environments is primarily driven by the relative red fraction, instead of the properties of the SF population \citep{muz12,koy13,lin14,wag17,jian17}. Using Pan-STARRS1 clusters \citep{lin14,jian17}, it is found that the specific star formation rates (sSFRs) of SF galaxies in the clusters are only moderately lower than those the field ($<$ 0.2-0.3 dex) and the difference becomes insignificant on groups scales. However, the uncertainty remains large for high mass galaxies because of the small sample sizes used in these studies, and it is also uncertain that the environmental quenching can extend to low mass galaxies.

In this work, we probe the properties of cluster galaxies using a large sample drawn from the HSC Subaru Strategic Program (hereafter the HSC survey). The HSC survey \citep{aih17} consists of three survey layers, `Wide', `Deep', and `UltraDeep' components. The cluster sample used in this work comes from the HSC CAMIRA (Cluster finding Algorithm based on Multi-band Identification of Red-sequence gAlaxies) catalog \citep{ogu17} constructed in the HSC Wide field, reaching $i \sim 26$ at 5$\sigma$ over 174 deg$^{2}$. It contains 4972 clusters with richness larger than 10 in the redshift range of $0.2 < z < 1.1$. This allows us not only to extend the analysis to redshifts greater than 0.8 and to fainter galaxy populations by 2 magnitudes in $i$, but also to increase the sample size by a factor of 17 compared to our previous works \citep{lin14,jian17}. There are two other companion papers in this special issue to address the environmental effects but using different catalogs and methods. \citet{koy17} make use of the NB emitter catalogs constructed for HSC-SSP Deep and UltraDeep fields to search for ``red emitter'' along the large-scale structures at 0.2 $<$ $z$ $<$ 1.7 and identify their environments. \citet{nis17} utilize the CAMIRA catalog to study the evolution of cluster profile for red and blue populations out to $z$ $<$ 1.1 and reveal the color-magnitude relation of red-sequence galaxies at the faint end $z$ $<$ 24.

Our paper is formatted as follows. In Section 2, we briefly describe the data, the sample selection, and the analysis method. In Section 3, we present the main results, discussing the main sequence properties, and the redshift and mass dependence of field, group, and cluster galaxy properties. In Section 4, our conclusion and discussion are presented. Throughout this paper we adopt the following cosmology: Throughout this paper we adopt the following cosmology: \textit{H}$_0$ = 100$h$~km s$^{-1}$ Mpc$^{-1}$, $\Omega_{\rm m} = 0.3$ and $\Omega_{\Lambda } = 0.7$. We adopt the Hubble constant $h$ = 0.7 when calculating rest-frame magnitudes. All magnitudes are given in the AB system.

\section{Data, Sample Selection, and Method}

\subsection{HSC Galaxy Sample}
Hyper Suprime-Cam (HSC) Survey is conducted as part of a 300-night Strategic Survey Program (SSP) over 5 years starting from March of 2014, aiming to explore the nature of dark matter and dark energy as well as the evolution of galaxies. The first public data of HSC-SSP are released recently \citep{aih17}. The Survey utilizes the wide field of view of 1.77 square degrees of Hyper Suprime-Cam to collect broad-band images in \textit{grizy} bands as well as to study emission line objects at high redshifts through a number of narrow-band filters \citep{aih17}.  HSC Survey consists of a three-layered imaging, including Wide, Deep, and UltraDeep. The aimed coverage for the Wide survey has 1,400 square degrees of the sky in all the five broad-band filters located around the equator and two large stripes around the spring and autumn equator with an additional stripe around the Hectomap region. The Deep survey is carried out in four separate fields; XMM-LSS, Extended-COSMOS (ECOSMOS), ELAIS-N1 and DEEP2-F3, and the UltraDeep has two fields, COSMOS and SXDS. The detail survey description can be found in \citet{aih17}.

In this study, we make use of the S16A photometric redshift catalog based on the S16A internal data release of the HSC Survey released in 2016 August. The HSC Wide S16A dataset contains imaging data taken between 2014 March and 2016 April in all five broad-bands at full depth and covers $\sim$ 174 deg$^2$. The HSC data is processed by the HSC Pipeline, or hscPipe (Bosch et al. 2017, in prep.), which is based on the Large Synoptic Survey Telescope pipeline \citep{ive08,axe10,jur15}. In addition, the HSC astrometry and photometry are calibrated against the Pan-STARRS1 3$\pi$ catalog \citep{ton12,sch12,mag13}. For more detail descriptions, readers are referred to \citet{aih17}.

\begin{figure*}
\includegraphics[scale=1.4]{f1.eps}
\caption{The images show the color-coded number densities of stacked galaxies for the SFR-M$_*$ relation in three redshift ranges from [0.2,0.5], [0.5, 08] to [0.8, 1.1] (from the top to the bottom)  and in three different environments, including the field (left), groups (middle), and clusters (right), respectively. The color scale in the color-bar is proportional to the number counts in each cell normalized by the cell with the maximum count. The diagonal lines represent the boundaries to separating star-forming and quiescent populations. They are sSFR = 10.1 in $0.2 < z < 0.5$, 10. in $0.5 < z < 0.8$, and 9.9 in $0.8 < z < 1.1$, respectively. The white solid lines with error-bars, estimated using the jack-knife resampling from eight sub-samples, denote the median values of SFRs at different stellar masses. We can qualitatively learn the redshift evolution of galaxies in three distinct environments, and at the same redshift, the differences of galaxy distributions in the SFR-M$_*$ space in different environments to see the environmental impact.}
\label{f1}
\end{figure*}

\subsection{CAMIRA Groups/Clusters}
The group/cluster sample is a product produced by a cluster-finding algorithm CAMIRA (Cluster finding algorithm based on Multi-band Identification of Red sequence gAlaxies) as described in \citet{ogu14}. Based on the stellar population synthesis (SPS) model of \citet{bru03}, CAMIRA fits all photometric galaxies for an arbitrary set of bandpass filters and computes likelihoods of being red-sequence galaxies as a function of redshift. To improve the accuracy of the model prediction, additional calibration is done through using a sample of spectroscopic galaxies to derive residual colors of SPS model fitting as a function of wavelength and redshift. The detailed methodology of the CAMIRA algorithm can be found in \citet{ogu14}.

In this work, we utilize a new optically selected CAMIRA cluster catalog from the first two years of observation of the HSC Survey, i.e. the HSC Wide S16A CAMIRA catalog \citep{ogu17}, to study galaxies properties in groups and clusters. The sample contains 4972 clusters/groups with richness $N_{mem}$ $>$ 10 in redshift range of 0.1 $<$ $z$ $<$ 1.1, and is validated through comparisons with spectroscopic and X-ray data as well as mock galaxy catalogs. It is shown in \citet{ogu17} that the redshift evolution of the mass threshold is not strong. That is, the constant richness cut roughly corresponds to the constant halo mass cut. Based on the cluster redshifts and the richness $N_{mem}$, we bin the clusters into three redshift ranges,  0.2 $<$ z $<$ 0.5, 0.5 $<$ z $<$ 0.8, and 0.8 $<$ z $<$ 1.1, to study their evolution and two richness ranges, 10 $<$ $N_{mem}$ $<$25 and $N_{mem}$ $>$ 25, to explore the ``group'' and ``cluster'' environment, respectively. Here $N_{mem}$ = 10 and 25 correspond to the virial halo mass log$_{10}$(M$_{vir}$/h$^{-1}$ M$_{\odot}$) $\sim$ 13.61 $\pm$ 0.13 and 14.19 $\pm$ 0.02, based on Equation 40 in \citet{ogu14}. Be noted that clusters with richness less than 15 are not included in \citet{ogu17} since these less massive clusters (or groups) suffer more contamination.

\begin{table}
\tbl{CAMIRA Cluster Catalog}{%
\begin{tabular}{cccc}
\hline\noalign{\vskip3pt}
\multicolumn{1}{c}{Redshift} & $z_{median}$ & Group & Cluster \\
\hline\noalign{\vskip3pt}
\multicolumn{1}{c}{} & & 10 $<$ $N_{mem}$ $<$ 25 & $N_{mem}$ $>$ 25 \\  [2pt]
\multicolumn{1}{c}{} & & M$_{vir}$/M$_{\odot}$ = 10$^{13.6-14.2}$ &  10$^{> 14.2}$ \\
\hline\noalign{\vskip3pt}
 0.2 $< z <$ 0.5  & 0.33 & 1139 & 194   \\
 0.5 $< z <$ 0.8  & 0.68 & 1506 & 153  \\
 0.8 $< z <$ 1.1  & 0.92 & 1611 & 95  \\
\hline\noalign{\vskip3pt}
\end{tabular}}\label{table:cataloginfo}

\end{table}

\begin{figure}
\includegraphics[scale=0.6]{f2.eps}
\caption{The median SFR of the SF main sequence in the field in redshift range of 0.2 $<$ $z$ $<$ 0.5 (purple), 0.5 $<$ $z$ $<$ 0.8 (green), and 0.8 $<$ $z$ $<$ 1.1 (blue) from this work (solid lines) and from \citet{whi12} (dashed lines), respectively. The results of the SF main sequence in the field from \citet{wag17} (red and black triangles), \citet{muz12} (yellow), and \citet{noe07} with upper and lower limits (blue dotted lines) are also included for comparisons. The purple, green, and blue arrows denote the mass completeness limit for SF galaxies at $z$ = 0.5, 0.8, and 1.1. Our results, in general, are in agreement with the results from literature. }
\label{f2}
\end{figure}

\subsection{The photo-z catalog and stellar mass estimation}

Photometric redshifts and physical properties of galaxies such as stellar mass and star formation rate are inferred using a photometric redshift code \texttt{Mizuki} \citep{tan15}. It is a template fitting code and templates are generated using \citet{bru03}. When deriving stellar masses and star formation rates, the Chabrier initial mass function (IMF) is assumed \citep{cha03}. The code applies a set of Bayesian priors on physical properties of galaxies in order to keep the model parameters within realistic ranges.  These priors are a function of redshift, which effectively let the templates evolve with redshift. It also applies template error functions to reduce systematic biases in the model templates and also to assign uncertainties to the templates. The code is run using the $grizy$ CModel photometry.  The redshift and physical parameters are estimated by marginalizing over all the other parameters. The quoted uncertainties in the physical properties thus include uncertainties in photometric redshifts.  Details of the calibration of the codes and the data products are described in the photo-z release paper (Tanaka et al. in prep.). It is also noted that there is a known bias in stellar mass in \texttt{Mizuki} which is about a factor of 2 larger than the mass in COSMOS at $z$ $\sim$ 1 \citep{tan15}.

\subsection{K-correction, Completeness Limit of Stellar Mass, and Star Formation Rate}
Our approach to computing the K-correction follows a similar method described in \citet{wil06} to relate the observed color and magnitude at redshift $z$ to the rest-frame color and magnitude based on empirical templates from \citet{kin96}. The detail description can be found in \citet{wil06} as well as in \citet{lin14}. In short, for a given redshift, we perform a polynomial fit between the K-correction term and a pair of adjacent observed color base on Kinney et al. templates, where the K-correction term is chosen to be the observed bandpass closest to the desired rest-frame quantity. Different input redshifts lead to different fitting results or polynomial formulas, and a table of fitting polynomial values can then be constructed and be applied to galaxies depending on their redshift in the range of 0 $<$ $z$ $<$ 1.45.

The estimation of the stellar mass limit follows the method described in \citet{lin14}.  We first compute the rest-frame quantities for galaxies at a given redshift based on their 5σ limiting magnitudes in the observed HSC bands utilizing the K-correction method illustrated previously. Adopting the empirical formula obtained by \citet{lin07}, we then convert the rest-frame magnitudes and colors to the corresponding stellar mass. It is known that at a fixed rest-frame magnitudes, the redder color a galaxy, the higher mass.  By taking the reddest colors of star-forming and quiescent populations, we derive their corresponding mass limits. In this way, we find that the mass limits log$_{10}$ (M$_*$ /M$_{\odot}$) are 8.6 (8.2), 9.3 (8.9), 9.7 (9.3) and 10.3 (9.8) for red (blue) galaxies at z $\sim$ 0.2, 0.5, 0.8, and 1.1, respectively.

\begin{figure*}
\includegraphics[scale=1.4]{f3.eps}
\caption{Best-fit parameters $\alpha$ and $\beta$ in Equation~\ref{equ1} for SF galaxies are plotted in three redshift ranges. This figure is based on the work by \citet{spe14}, who compile and calibrate the best-fit parameters from literatures including \citet{elb07}, \citet{noe07}, \citet{dun09}, \citet{san09}, \citet{oli10}, \citet{kar11}, \citet{whi12}, \citet{zah12}, and \citet{sob14}. Additionally, we add the results from \citet{wag17}, \citet{jian17} and this work. The best-fit parameters from \citet{whi12} are without uncertainties and shown by open circles.}
\label{f3}
\end{figure*}

We compute the SFR following the approach described in \citet{mos12}. The SFR is parameterized as functions of rest-frame optical B magnitudes M$_B$ and (U-B) color and calibrated against SED-fit SFR  from UV/optical bands in the All-Wavelength Extended Groth Strip International Survey for both red sequence and blue cloud galaxies in the 0.7 $<$ $z$ $<$ 1.4 redshift range. The calculated SFRs are found to agree well with an L[O$_{\rm{II}}$]-M$_B$ SFR calibration commonly used in the literature by considering a correction for the measured values M$_B$ from DEEP2 galaxies to include a dimming factor of Q = 1.3 magnitudes per unit redshift \citep{mos12}. In this work, we adopt the fitting formula using the rest-frame optical M$_B$, (U-B), and a second order (U-B) color as fit parameters and the fit coefficients can be found in Table 3 in \citet{mos12}. It is reported in \citet{mos12} that the SFR uncertainties depend on colors of galaxies. Although the method gives more precise SFRs for star-forming galaxies and less accurate SFRs for quiescent ones, it uncovers the SFR of galaxies with a wide range of star formation activities. In this study, the main emphases are the comparisons of star formation rate for star-forming galaxies and the quiescent fraction in different environments. The larger uncertainty in the SFR estimate for quiescent objects has little impact on our results.

The sSFR, defined as SFR/M$_*$, is used to separate star-forming and quiescent populations. In this work, the separating thresholds we apply are log$_{10}$(sSFR) = -10.1 yr$^{-1}$ in $0.2 < z < 0.5$, -10.0 yr$^{-1}$ in $0.5 < z < 0.8$, and -9.9 yr$^{-1}$ in $0.8 < z < 1.1$.

\subsection{Method}

By construction, the CAMIRA cluster catalog only contains red cluster members. In order to probe the properties of general populations in clusters, we perform the stacking analysis and correct for the background/foreground contaminations. The details of the method are discussed and illustrated in \citet{jian17}.  In short, the contaminated galaxy properties around the cluster centers during stacking can be statistically removed by subtracting the same galaxy properties of a mean local background, selected either from random positions or from annuluses between $r_1$ and $r_2$, where $r_1$ and $r_2$ are the inner and the outer comoving radii around cluster centers, respectively. For each cluster, we project galaxies around its center onto a plane within a redshift width equal to the photo-$z$ accuracy of the galaxy sample, i.e. $|z - z_{\textrm{grp}}| \leq \sigma_{\Delta z/(1+z_s)}$, where $z$, $z_{\textrm{grp}}$, and $\sigma_{\Delta z/(1+z_s)}$ are galaxy, group redshift, and photo-$z$ accuracy, respectively. For galaxies on this projected plane, their redshift is adjusted to the cluster redshift for k-correction. Galaxies within a projection radius $r_p$ 1.5 $\textrm{Mpc}$ from the center are considered as the contaminated cluster galaxy sample. The corrected sample can be obtained by subtracting the contaminated cluster galaxy sample with an area-normalized background sample. In this work, we select comoving $r_1$ and $r_2$ to be 8.0 and 10.0 $\textrm{Mpc}$, respectively.

\begin{figure*}
\includegraphics[scale=0.6]{f4.eps}
    \caption{Top: The median sSFR of SF galaxies as a function of redshift in the field (dotted), groups (dashed), clusters (solid), respectively. Bottom: The logarithmic ratio of sSFR for group to field galaxies (dashed), and for cluster to field galaxies (solid). In addition, the red and cyan circles denote the sSFR of SF galaxies in the field from \citet{alb14} for M$_*$ $>$ 1.3 $\times$ 10$^{10}$ M$_{\odot}$ and in clusters from \citet{wag17} for M$_*$  $>$ 10$^{10.1}$ M$_{\odot}$, respectively. The yellow shade region gives the boundaries of the infrared Main Sequence as defined in \citet{elb11}. In the upper left panel, the data points in the redshift range of 0.8 $<$ $z$ $<$ 1.1 for the mass bin 9.5-9.75 are removed due to the mass incompleteness. The trend that the sSFR decreases with the decreasing redshift and the decreasing level for the same redshift range in our results are in good agreement with other works although a systematics is seen.}
\label{f4}
\end{figure*}

\section{Results}
\subsection{Main Sequence Properties}
The main sequence indicates the tight correlation between galaxy SFR and M$_{*}$ for star-forming (SF) galaxies.  In Figure~\ref{f1}, we show the  color-coded number density plots of stacked galaxies for the SFR-M$_{*}$ relation in 3 redshift bins,[0.2,0.5], [0.5,08] and [0.8,1.1] (from the top to the bottom), and in the environment of the field (left), groups (middle), and clusters (right). The diagonal dashed lines separate the star-forming or the main sequence (above) and quiescent galaxies (below) with log$_{10}$(sSFR) = -10.1 yr$^{-1}$ in $0.2 < z < 0.5$, -10.0 yr$^{-1}$ in $0.5 < z < 0.8$, and -9.9 yr$^{-1}$ in $0.8 < z < 1.1$. The colors are scaled with the number counts in each cell normalized by the cell with the maximum count. The solid white lines with error-bars give the median SFRs of SF galaxies in different redshifts and environments as a function of the stellar mass. The error-bars are estimated from eight sub-samples using the jack-knife resampling method. It is seen that the distributions of field galaxies have a distinct appearance from those of group or cluster galaxies. In the field, the presence of star-forming galaxies is so prominent that quiescent galaxies can almost be neglected for all masses. By contrast, in groups or clusters, quiescent galaxies become the dominant ones for mass roughly larger than 10$^{9.5-10}$ $M_{\odot}$. In general, our results are in good agreement with the conclusions from previous studies that the group or cluster environment has a higher red fraction of galaxies than the field environment \citep{ger07,gio12}. In addition, the evolution of field, group, and cluster galaxies can also be seen clearly. Qualitatively, the main sequence of SF field galaxies has lower sSFR as it evolves from high redshift to low redshift. The fraction of the quiescent population in groups and clusters becomes higher with the decreasing redshift, and at the same redshift, the quiescent population in clusters is more prominent than in groups, evident the hosting environmental effect.

\begin{figure*}
\includegraphics[scale=0.6]{f5.eps}
\caption{The redshift evolution of the quiescent fractions ($f_q$s) for field (dotted), group (dashed), cluster (solid) galaxies, respectively.  Similar to the upper left panel in Figure~\ref{f4}, the data points in the high redshift bin for the mass bin 9.25-9.5 are removed due to the mass incompleteness. The Butcher-Oemler effect \citep{but84} is clearly seen but with a mass dependence. The effect is stronger for less massive galaxies and less for massive galaxies. For comparisons, we also add the $f_q$ results from \citet{wag17} (cyan circles) with M$_*$  $>$ 10$^{10.1}$ M$_{\odot}$ in the upper right panel. It is seen that our result is in agreement with that from \citet{wag17}. }
\label{f5}
\end{figure*}

To further quantitatively understand our results, the main sequence at different redshift is compared with that from \citet{whi12} in Figure~\ref{f2}. The purple, green, and blue solid lines represent the median SFR in three redshift ranges from low to high redshift in our sample, respectively. The three dashed lines plot the fitting lines at median redshifts in our three bins, $z_{med} = $ 0.33, 0.68, and 0.93, using the best-fit parameters from \citet{whi12}. We adopt the mass conversion factors from \citet{spe14} for stellar mass assuming different initial mass function (IMF), i.e., M$_{*,K}$  = 1.06 M$_{•,C}$ = 0.62 M$_{*,S}$, where S, C, and K, are referred to Salpeter, Chabrier, and Kroupa IMFs. The dotted blue line gives the best-fit results from \citet{noe07} in 0.2 $<$ $z$ $<$ 0.7. The yellow diamonds with error-bars are the SFRs of SF cluster galaxies in redshift range between 0.15 and 0.8 from \citet{muz12}, and the black and red triangles represent the SFRs of SF cluster galaxies in 0.15 $<$ $z$ $<$ 0.8 and 0.8 $<$ $z$ $<$ 1.5, respectively. It is seen that the best-fit slopes and magnitudes of the SF main sequence in our sample in three redshift ranges agree well with those in \citet{whi12} and \citet{noe07}, and are in broad agreement with those from \citet{wag17}. Additionally, we quantify the main sequence by fitting the data with a formula of a power law, i.e.
\begin{equation}\label{equ1}
log_{10}(\rm{SFR}/M_{\odot}   yr^{-1}) = \alpha log_{10}(M_*/M_{\odot}) + \beta,
\end{equation}
where $\alpha$ and $\beta$ are the slope and normalization, respectively.  In Figure~\ref{f3}, our best-fit $\alpha$ and $\beta$ for SF field galaxies in three different redshift ranges are plotted with a selection of literature best-fit parameters from a sample of 25 studies in the redshift range of 0 $<$ $z$ $<$ 6, compiled and calibrated by \citet{spe14}, including \citet{elb07}, \citet{noe07}, \citet{dun09}, \citet{san09}, \citet{oli10}, \citet{kar11}, \citet{whi12}, \citet{zah12}, and \citet{sob14}. All the above published best-fit parameters are standardized to a Kroupa IMF in \citet{spe14}. Besides, we add the results from \citet{wag17} for SF cluster galaxies, and from \citet{jian17} for SF field galaxies.  Our best-fit parameters are in good agreement with those from other published works, indicating the robustness of our results.

\begin{figure*}
\includegraphics[scale=0.6]{f6.eps}
\caption{Similar to Figure~\ref{f4} and \ref{f5}, the quenching efficiency $\varepsilon$ is plotted as a function of redshift for different mass ranges in four panels for field (dotted), group (dashed), and cluster (solid) galaxies, respectively. In general, the slope of the quenching efficiency decreases with the increasing masses, implying that the quenching effect is stronger for less massive galaxies.  }
\label{f6}
\end{figure*}

\subsection{Redshift Dependence}

\subsubsection{sSFR of SF galaxies, sSFR$_{\rm{SF}}$($z$)}
There have been many previous studies to discuss and compare the evolution of the main sequence in different environments \citep{koy13,lin14,erf16,wag17,jian17}. Taking the advantage of the large and deep HSC sample, we are able to explore the same subject with better statistics and low mass galaxies.  In Figure~\ref{f4}, the median sSFRs of the star-forming galaxies in field (dotted lines), group (dashed lines), and cluster (solid line) environments on the top, and the sSFR ratio of group to field galaxies (dashed lines) and that of cluster to field galaxies (solid lines) on the bottom are plotted as a function of redshift in different mass ranges separated in four panels. The yellow shaded region denotes the infrared main sequence as defined in \citet{elb11}, and is in the range of 13(13.8 Gyr - t )$^{-2.2}$ $<$  sSFR  $<$ 52(13.8 Gyr - t )$^{-2.2}$, where t is the look-back time. The red data circles mark the sSFR of the star-forming galaxies in the field from \citet{alb14} with stellar mass limit M $>$ 1.3 $\times$ 10$^{10}$ M$_{\odot}$. Four cyan circles with error-bars are from \citet{wag17} for SF cluster galaxies with mass larger than log$_{10}$(M$_*$/M$_{\odot}$) = 10.1. From Figure~\ref{f4}, our results show good consistency with that in \citet{elb11} and slightly shallower at low $z$ than that in \citet{alb14}.  It is seen that the decrease of the sSFR of the SF main sequence for field galaxies is $\sim$  0.45 dex from $z$ = 1.1 to 0.2 for all mass bins, possibly due to a global decline in the gas contents. At fixed masses, the decrease level is very similar to cluster and group galaxies between the same redshift range but a systematics is seen $<$ 0.4 dex for clusters and $<$ 0.2 dex for groups. That is, the decrease of sSFRs for the group to field galaxies and for the cluster to field ones is independent of redshift. However, the decrease appears to depend on stellar mass, being larger for less massive galaxies. Our results are in agreement with those in \citet{koy13} that the difference in the SFR-M$_*$ relation between cluster and field SF galaxies is $\sim$ 0.2 dex since $z$ $\sim$ 2.

\begin{figure*}
\includegraphics[scale=0.6]{f7.eps}
\caption{Similar to Figure~\ref{f4}, but the sSFRs of SF galaxies are shown as a function of stellar mass. In the upper left panel, the sSFR of SF field galaxies in redshift range of 0.2 $<$ $z$ $<$ 0.5, 0.5 $<$ $z$ $<$ 0.8, and 0.8 $<$ $z$ $<$ 1.1 is represented by the dashed, solid, and dotted line, respectively. The other three panels plot the sSFRs of SF field (black pluses), group (blue squares), and cluster (green circles) galaxies on the top, and the logarithmic ratio of sSFR for group to field galaxies (blue squares), and for cluster to field galaxies (green circles) on the bottom. For comparisons, we also include the sSFR results from \citet{lin14} in the redshift range of 0.5 $<$ $z$ $<$ 0.8 for SF field (red pluses), group (red squares), and cluster (red circles) galaxies. In addition, the sSFR results are added as well from \citet{muz12} for SF field (purple pluses) and cluster (purple circles) galaxies in redshift range of 0.85 $<$ $z$ $<$ 1.2, and from \citet{wag17} for SF cluster galaxies (cyan circles) in redshift range of 0.15 $<$ $z$ $<$ 0.8 (bottom left) and 0.8 $<$ $z$ $<$ 1.5 (bottom right).
\label{f7}
\end{figure*}

\subsubsection{Quiescent Fraction, $f_q$($z$)}
Under the stellar mass control, the redshift dependence of the quiescent fractions ($f_q$ )for field (dotted lines), group (dashed lines), and cluster (solid lines) galaxies is explored in Figure~\ref{f5}.  For comparison, the results from \citet{wag17} (cyan circles) with M$_*$ $>$ 10$^{10.1}$ M$_{\odot}$ are also plotted in Figure~\ref{f5}. Globally, the $f_q$ increases with decreasing redshift, consistent with the Butcher-Oemler effect \citep{but84}. However, depending on the galaxy masses, their effect can be significantly different. For high-mass galaxies, the Butcher-Oemler effect is weak and nearly negligible. On the other hand, the effect is stronger for low-mass ones, consistent with results in \citet{li12}.  For low-mass galaxies, the increase of $f_q$ is about 3 times larger from high $z$ $\sim$ 0.95 to low $z$ $\sim$ 0.35. In addition, the cluster downsizing effect that clusters with larger halo mass show greater quiescent fraction is also evident in our sample.   Our redshift evolution trend is similar to that in \citet{wag17},   and the $f_q$ derived for our sample in log$_{10}$(M$_*$/M$_{odot}$) = 10.2-10.5 (the blue solid line in upper right panel) appears to also be consistent with those in \citet{wag17}.

\subsubsection{Quenching Efficiency, $\varepsilon$($z$)}
We also compute the environmental quenching efficiency, $\varepsilon^{\textrm{envi}}$ = ($f^{\textrm{cluster}}_{q} - f^{\textrm{field}}_{q}$)/(1 - $f^{\textrm{field}}_{q}$), similar to the definition in \citep{pen10}, as a function of redshift in different mass bins to quantify the excess of quenching due to pure environmental effects in Figure~\ref{f6}.  In general, the quenching efficiency increases with the decreasing redshift, and also increases with the increasing mass at fixed redshift. However, the slope of the quenching efficiency decreases with the increasing masses, implying that the quenching effect is stronger for less massive galaxies. The redshift dependence becomes weaker for the high-mass galaxies, likely due to being red and dead already for most of the massive galaxies at high redshifts.  In addition, it is seen that the environmental quenching in clusters is larger than that in groups, indicating that the hosting environment has a significant effect on the star formation quenching.

\begin{figure*}
\includegraphics[scale=0.6]{f8.eps}
\caption{The quiescent fraction $f_q$s as a function of stellar mass. In upper left panel, the f$_q$s are plotted for field galaxies in three redshift bins while the other three panels show the f$_q$s of field (black pluses), group (blue squares), and cluster (green circles) galaxies in redshift range of 0.2 $<$ $z$ $<$ 0.5 (upper right), 0.5 $<$ $z$ $<$ 0.8 (bottom left), and 0.8 $<$ $z$ $<$ 1.1(bottom right). The red pluses, squares, and circles denote the $f_q$s for field, group, and cluster galaxies, respectively, from \citet{lin14} in redshift range of 0.5 $<$ $z$ $<$ 0.8. The cyan circles are data points from \citet{wag17} for cluster galaxies in redshift range of 0.15 $<$ $z$ $<$ 0.41 (upper right), 0.41 $<$ $z$ $<$ 0.8 (bottom left) and 0.8 $<$ $z$ $<$ 1.5 (bottom right). The purple pluses and circles represent the $f_q$s for field and cluster galaxies, respectively, from \citet{muz12} in redshift range of 0.85 $<$ $z$ $<$ 1.2.}
\label{f8}
\end{figure*}

\subsection{Stellar Mass Dependence}
\subsubsection{sSRF of SF galaxies, sSFR$_{\rm{SF}}$(M$_*$)} \label{ssfr_ms}
In Figure~\ref{f7}, the sSFRs of SF galaxies are plotted as a function of the stellar mass M$_{*}$ in different hosting environments and redshift ranges. In the upper left panel, the median sSFR of SF field galaxies is shown in redshift range of 0.2 $<$ $z$ $<$ 0.5 (dashed line), 0.5 $<$ $z$ $<$ 0.8 (solid one), and 0.8 $<$ $z$ $<$ 1.1 (dotted line) for comparisons, respectively. For the other three panels on top-right, bottom-left, and bottom-right, the sSFRs of SF field (black pluses), group (blue squares), cluster (green circles) galaxies are plotted on the top while the logarithmic ratio of sSFR for SF group to field galaxies (blue squares) and that for SF cluster to field ones (green circles) are displayed on the bottom. Additionally, the red pluses, squares, and circles denote the sSFR of SF field, group, and cluster galaxies in 0.5 $<$ $z$ $<$ 0.8 from \citet{lin14}, respectively. The cyan circles are the sSFRs of SF cluster galaxies in 0.15 $<$ $z$ $<$ 0.8 and in 0.8 $<$ $z$ $<$ 1.5 from \citet{wag17}, and the purple pluses and circles are those of SF field and cluster galaxies in 0.85 $<$ $z$ $<$ 1.2 from \citet{muz12}.

In general, the median sSFR of group or cluster galaxies decreases from that of field ones, implying a slow quenching effect acting in dense environments. We found that there is a weak dependence on the stellar mass of the sSFR deficit relative to the field, which is $<$ 0.2 dex in groups and  $<$ 0.4 dex in clusters. The larger deficit seen in cluster galaxies as opposed to group galaxies suggests a stronger environmental quenching effect in clusters than in groups. It is worth noting that the decreases are slightly larger from what was found in \citet{lin14}, who found no significant sSFR reduction of SF galaxies in the groups and $\sim$ 17 $\%$ (0.23 dex) sSFR decrease for the SF galaxies in the clusters relative to the field galaxies. However, we note that the halo mass binning is 10$^{13.6-14.2}$ M$_{\odot}$ for groups and 10$^{ > 14.2}$ M$_{\odot}$ for clusters in this work while it is 10$^{13.4-14.0}$ M$_{\odot}$ for groups and 10$^{> 14.0}$ M$_{\odot}$ for clusters in \citet{lin14}. The larger sSFR offset seen in this work may be attributed to the greater masses of the groups and clusters probed in our analysis, since larger sSFR reduction is expected in more massive clusters. In addition, less massive groups normally suffer from the more serious foreground and background contaminations and the real group signals can be easily smeared out, leading to the less sSFR reduction. In the high redshift (bottom-right) panel, although there seems to have a systematic between our results and the results from \citet{muz12} and \citet{wag17} for the absolute sSFR values, the decreasing trend of the sSFR with the increasing mass in our sample agrees well with them. Besides, it is noticed that our results for the sSFR reductions are in broad agreement with those from \citet{muz12}.

\begin{figure*}
\includegraphics[scale=0.6]{f9.eps}
\caption{The quenching efficiency $\varepsilon$s as a function of stellar mass. Similar to Figure~\ref{f7} and \ref{f8}, the $\varepsilon$s of field galaxies in three redshift bins are shown in the upper left panel while the other three panels plot the $\varepsilon$s of field (black pluses), group (blue squares), and cluster galaxies (green circles) in three redshift ranges, respectively. It is clearly seen that the transition masses from the dominance of the environment quenching to that of the mass quenching are log$_{10}$(M$_*$/M$_{\odot}$) $\sim$ 10.4 in groups and $\sim$ 10.6 in clusters.}
\label{f9}
\end{figure*}

\subsubsection{Quiescent Fraction, $f_q$(M$_*$)}
The quiescent fraction ($f_q$) is investigated as a function of $M_*$ in Figure~\ref{f8}. Similar to Figure~\ref{f7}, the upper-left panel shows the $f_q$ for field galaxies in three redshift ranges, and the other three panels give the comparisons of $f_q$ for the field, group, and cluster galaxies in one redshift range per one panel. Results of $f_q$ are included for comparisons from \citet{muz12} for field and cluster galaxies in redshift range of 0.85 $<$ $z$ $<$ 1.2, from \citet{lin14} for field, group, and cluster galaxies in 0.5 $<$ $z$ $<$ 0.8, and from \citet{wag17} for cluster galaxies in 0.15 $<$ $z$ $<$ 0.41, 0.41 $<$ $z$ $<$ 0.8, and 0.8 $<$ $z$ $<$ 1.5. It is seen that the quiescent fraction depends strongly on mass and less strongly on redshift and the hosting environment. At high redshifts, the $f_q$ difference at fixed mass between group and cluster galaxies is small and gradually becomes larger with the decreasing redshift, indicating that the environmental quenching effect has a redshift dependence.  In addition, the typical "downsizing" effect in which less massive galaxies are more star-forming continues down to $\sim$ $10^{9}$ M$_{\odot}$. Moreover, at low mass, it is found that the red sequence is still visible in groups or clusters with respective to the field, implying that the environmental quenching can still effectively stop star-formation for low mass galaxies. It is noticed that the $f_q$ in this work is higher compared to those from \citet{lin14} and \citet{wag17}. Besides the greater cluster masses used in this work (see the discussion in the previous section \ref{ssfr_ms}), it is also likely that the CAMIRA cluster finding is based on the red sequence method and preferentially select clusters with high $f_q$. In the high redshift range,  our $f_q$s broadly agree with those from \citet{muz12}. However, lower $f_q$s are found in \citet{wag17}, likely due to the fact that their sample includes galaxies up to $z$ $\sim$1.5.

\subsubsection{Quenching Efficiency, $\varepsilon$(M$_*$)}
The environmental quenching efficiency is schemed as a function of stellar mass in Figure~\ref{f9} in order to better quantify the excess of quenching due to pure environmental effects. The panel arrangement is similar to that in Figure~\ref{f7} and \ref{f8}. In the upper-left panel, the quenching efficiency from field galaxies, or the mass quenching efficiency assuming that field galaxies are purely quenched by their masses, are displayed in three redshift ranges. The other three panels present the comparisons among the field, group, and cluster galaxies per redshift bin. It is clearly seen that both the mass and environmental quenching increases with increasing stellar mass. However, high mass galaxies are dominated by the mass quenching while low mass galaxies are quenched primarily due to the environmental quenching. The transition mass where the dominance of the mass and environmental quenching switches is recognized at log$_{10}$(M$_*$/M$_{\odot}$) $\sim$ 10.4 in groups and 10.6 in clusters in the lowest redshift range of $0.2 < z < 0.5$, in good agreement with the results from \citet{lin14}.  This implies that the environmental quenching in clusters is more prominent than that in groups since it can quench more massive galaxies than in groups.

\section{Conclusion and Discussion}
In this work, we probe galaxies down to $i \sim$ 26, two magnitudes deeper than that in our previous works \citep{lin14,jian17}, and extend our results to redshift 1.1, enabling us to study the cosmic evolution of the star formation activity. Due to the exceptional deep depth of our sample, the stellar mass completeness limit can be pushed to log$_{10}$(M$_*$/M$_{\odot}$) = 9.8 and 10.3 at $z$ $\sim$ 1.1 for star-forming and quiescent galaxies, respectively. That is, we are able to explore the quenching status of lower-mass star-forming galaxies which have not explored in our previous works. Additionally, the HSC Wide 16A data are collected from a survey area $\sim$ 174 square degree to offer good statistics even for galaxies at the high-mass end. In other words, we can constrain the results on high mass galaxies more robustly as opposed to previous studies. The main results can be summarized below:

1. The sSFR of star-forming galaxies decreases with cosmic time, regardless the environments. The sSFR is lower in groups and clusters than in the field by $\sim$0.1 dex and $\sim$0.2--0.3 dex, respectively. The drop of sSFR in group/cluster environments is insensitive to the redshift and is more significant for low mass galaxies.

2. The quiescent fraction is a strong function of stellar mass in all environments, being greater for higher mass galaxies. The Butcher-Oemler effects are seen in all environments and are more prominent for low mass galaxies.

3. Both the environment and stellar mass quenching efficiencies increase with the stellar mass. However, the environment quenching dominates over the stellar mass quenching for low mass galaxies.

At a fixed stellar mass, we find that the decrease in the sSFR of star-forming group or cluster galaxies to field ones is 0.1-0.3 dex and is more prominent in cluster environments. This implies that galaxies in clusters likely experience a long timescale (or slow) quenching effect that gradually reduces the SFR of star-forming galaxies. Although the gas contents and hence the star formation rate of galaxies vary with redshifts, we find that the offsets in the sSFR in groups/clusters, as opposed to the field, are comparable at different redshifts, in agreement with the results found by \citet{koy13}. This implies that the slow quenching mechanism acting on groups/clusters is likely universal in the redshift range of $0.2 < z < 1.1$.

In addition, it is found in this work that the transition masses from environment quenching to the mass quenching are 10$^{10.4}$ M$_{\odot}$ and 10$^{10.6}$ M$_{\odot}$  in groups and clusters, respectively, in the lowest redshift bin of $0.2 < z < 0.5$, in good agreement with the results from \citet{lin14}. The greater transition mass in clusters suggests that the environment effects are more important in clusters than in groups and have an effect even for massive galaxies. It is also noticed that the red fraction for the most massive galaxies is comparable between the field and group/cluster environments. This suggests that the star formation of those massive galaxies beyond the transition mass are likely already stopped and being red and dead before they enter the cluster-like environments. Conversely, the environmental quenching dominates the mass quenching in low mass galaxies below the transition mass in groups or clusters down to the mass completeness limit of 10$^{8.6}$ M$_{\odot}$ at $z$ $\sim$ 0.2, and the environmental quenching effect in clusters is stronger than that in groups. At this low mass regime, the red sequence is still visible in groups or clusters with respective to the field, suggesting that the environmental quenching can still effectively stop star-formation for low mass galaxies.

\citet{koy17} recently present their results discussing the environmental dependence of color, stellar mass, and sSFR of H$_{\alpha}$-selected galaxies in twin clusters in the DEEP2-3 field at $z$ = 0.4. One import finding in their work is that H-selected galaxies reveal color-density or color-radius correlations, but their stellar masses or sSFRs are independent of environments. The conclusion appears to be inconsistent with our result that there is a systematical reduction of sSFR for SF galaxies in groups or clusters by 0.1 - 0.3 dex with respect to those in the field. As discussed in \citet{koy17}, there are various factors that may contribute to this discrepancy. It is likely due to different definitions for SF galaxies in our and their sample. Our SF galaxies are determined by their sSFRs while SF galaxies are detected as H$_{\alpha}$ galaxies in \citet{koy17}. In addition, it is indicated that the treatment of dust extinction or NII line contamination could easily change the results by $>$10-20$\%$ level, which can significantly ease the inconsistency between us. Finally, it is also possible that the sample size of H$_{\alpha}$ emitters in \citet{koy17} is much smaller than that of our sample, which covers whole HSC S16A Wide survey area, and poor statistics (particularly in a high-density environment) may lead to the disagreement in conclusions.

\begin{ack}

This work is supported by the Ministry of Science \& Technology of Taiwan under the grant MOST 103-2112-M-001-031-MY3 and MO is supported in part by World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan, and JSPS KAKENHI Grant Number 26800093 and 15H05892. The Hyper Suprime-Cam (HSC) collaboration includes the astronomical communities of Japan and Taiwan, and Princeton University.  The HSC instrumentation and software were developed by the National Astronomical Observatory of Japan (NAOJ), the Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU), the University of Tokyo, the High Energy Accelerator Research Organization (KEK), the Academia Sinica Institute for Astronomy and Astrophysics in Taiwan (ASIAA), and Princeton University.  Funding was contributed by the FIRST program from Japanese Cabinet Office, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), the Japan Society for the Promotion of Science (JSPS),  Japan Science and Technology Agency  (JST),  the Toray Science  Foundation, NAOJ, Kavli IPMU, KEK, ASIAA,  and Princeton University.
\end{ack}

redpajama_set_name: RedPajamaArXiv


The responsible design of financial products is a topic of increasing regulatory interest (ASIC, 2014). The issues range from the performance and risks of complex financial instruments, to the marketing and advertising of products to consumers (OECD, 2013). In this research, the relationship of financial literacy to product design is examined in the context of known behavioural finance anomalies. The choice of words used to position a product on the risk-reward spectrum is examined in the context of complex financial products. The study employs semiotic analysis, a method originally from literary criticism, which is now applied to consumer choice (Mick, 1986), advertising (Adams & García, 2007) and the analysis of messaging in audit reports (Hronsky, 1998) and credit risk (Bonne, 2011). This paper finds evidence of a misleading framing of risk and reward in the advertising for binary options. Our recommendation is to consider tighter guidelines on the use of language like investments, when dealing with instruments which are clearly speculative, with the financial properties of gambles.


text:
"Ys" Series Review Part 7: "Ys Seven"
Shaun Mudd
Shaun is a writer and game collector with a wide variety of games from different generations. He likes reviewing some of the games he owns.
Welcome to the seventh and currently final part of the Ys Series Review. In this part, we will be talking about the seventh game in the Adol story and the eighth overall, a game known as Ys Seven. Yes, the title is literally "Seven" spelled out. Seven has the greatest departure in gameplay yet and has perhaps had the greatest impact of all of the recent Ys games. That departure is what we will be looking at today. Some spoilers lie ahead, so proceed at your own risk.
Ys Seven was released on the PlayStation Portable in Japan in September of 2009, followed by a North American and European release in 2010. The only thing about the European release is that it is exclusive to the PlayStation Store. Outside of a Chinese PC release in 2012, this game remained a PSP exclusive, though playable on the Vita and PlayStation TV, for the longest time until August 30, 2017 when a separate PC port was released by XSeed on Steam and GOG.
The world of Ys Seven is bigger than the world of any Ys game that was made up to that point and has only been surpassed by the likes of Memories of Celceta and Ys VIII. Speaking of Memories of Celceta, if you saw my article discussing that game, you may have noticed that I did not really go into detail about the gameplay of that game. That is because the gameplay in that game is based on what is seen in Ys Seven. What is so special about Ys Seven's gameplay, you might ask? The game revolves around a party system where you get to play as different characters with different weapons and attack types to get through the game. This is a stark difference in comparison to all of the Ys games that came before where you only play as Adol through the entire game. The only exception is Origin where there are three characters, but that was still a solo adventure.
Now the gameplay of Ys Seven might seem different at first glance, but the different attack types are nothing that has not been seen before in the likes of Oath in Felghana and Ark of Napishtim. The only significant difference between this and using bracelets and different swords respectively is that you have a different character model to go with it. Most of the characters are memorable and enjoyable, and a few familiar faces from past games return such as Geis and arguably the second main character of the Ys series, Dogi, who is finally playable after so many years.
Adol on the seas.
The plot of Ys Seven may be the longest seen up to the point when it was released. It is set about six months after the events of The Ark of Napishtim and starts as Adol and Dogi are on a ship heading to the country of Altago, a country they were unable to reach earlier thanks to a war with the Romuns that was mentioned in Ark of Napishtim and some newer games like Memories of Celceta. Thanks to a recent ceasefire, it is now possible to travel between the two countries though some of the people are still tense from the conflict.
Shortly after landing in Altago, Adol and Dogi have a run-in with one of Altago's Dragon Knight commanders who is causing trouble for one of the local girls, and this commander has Adol and Dogi imprisoned as suspected Romun spies. They are bailed out by the king of Altago, who happens to be a friend of Ladoc, and he sends them to travel throughout the land and investigate the recent increase in monsters and disasters such as earthquakes. So, they travel around Altago where they meet members of the five tribes of Altago, each of whom is watched over by a powerful dragon.
I think most of us saw this joke coming.
Adol is chosen as the dragon warrior who must receive the power of all five dragons so he can prevent a ritual that will destroy all of Altago. He is assisted by members of the elder families off all five tribes with one of the main characters being the princess of Altago.
Missing sanctuary, eh? It couldn't possibly be this huge stone in the middle of the-
Finding the sanctuaries where four of the dragons are is easy since four of the tribes still exist, but the one for the Moon Tribe is more of a challenge since their elder line disappeared long ago along with knowledge of the sanctuary. They eventually do, however, and learn that this ritual has happened many times throughout the ages with countless dragon warriors who had failed. Since this is Adol's game, there is no way he can fail and he does succeed in stopping the ritual and destroying the source, ending it for all time. Altago has to be rebuilt after the recent disasters and Adol and Dogi stay for a bit to help out, but they eventually continue on their adventures. There are many more plot points and twists, but those are best saved for when you play the game.
Ys Seven has had a pretty big impact on the Ys series, which is interesting given that Falcom was not sure how well the party system would be received and they had a second version of the game planned in case the reception was negative, though that version was not needed as it proved to be a popular system that likely will not be going anywhere in the near future. The popularity of the party system in Ys Seven is apparent since it has been featured in both of the Ys games that have been made since the release of Seven in 2009. That includes the reimagining of the fourth game, Memories of Celceta, and the recently released Ys VIII. Both have taken the gameplay of Seven and greatly improved and refined it. While some have not been thrilled with the party system since they prefer Adol working on his own, many others including myself like the party system and the extra dynamic it adds, not to mention all of the unique characters these games have that might not have been possible before. Even with the different characters to play as, it is always clear that Adol is the central character in all of these games and that likely will not change anytime soon, if ever.
However, there is one thing this game did from a plot perspective that I thought was rather strange. When Adol and Dogi sail into Altago Dogi mentions Adol's bad luck with ships and seems to turn that into something of a running joke. Let's look at how many times Adol was shipwrecked in the series, shall we?
How many times has Adol been shipwrecked?
How Game begins
Ys I & II
The Oath in Felghana
Lands safely
Memories of Celceta
Ys V
Ark of Napishtim
Ys Seven
Ys VIII (Might as well include this here)
So out of all seven of Adol's main adventures he gets involved in a shipwreck three times, a little under half of the time. And one of the games where he was shipwrecked didn't even exist at the time! I guess that could work as a running gag, but he still arrives safely most of the time. It is still strange though to make a running gag out of something that has only happened a couple of times. That is all I have to say on Ys Seven. My final verdict for this excellent game is:
8/10 (Great)
If you ever get the chance I highly recommend playing this game. There are only a few options available to play this game since it is recent enough. As mentioned earlier, it was released digitally on the PSP so it is also playable on the Vita and PS TV if you happen to have any of those, and it is now available on PC worldwide. I hope you enjoyed this look at all of the games in the incredible Ys series. This is all there is for now, but I will be looking at the eighth game after it is released worldwide. See you then.

redpajama_set_name: RedPajamaCommonCrawl


Do You Really Want to Meet an Orca?
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text:
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Request this hotel
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text:
Q: custom url for custom module in Drupal? I am new to Drupal development. So..I have created a new module and named it as 'apps'.
The module simple queries a node from my database and display it. To access this module, I access http://domain/apps/1 where 1 is a node id.
My question is,
how do I change 'apps' to something else without changing the module name?

A: A path like that is defined in hook_menu(), in your case that should be in the function apps_menu(). You can simply use another path, although it is recommended to stay inside the namespace of your module to avoid conflicts with other modules (see comments for more information).

A: Use "path" module, it's included in drupal distr., then create manually association "apps" to something other alias. Pathauto also will useful if you want automate paths aliasing.

A: It seems you can also use a wildcard loader argument.
If you put %node in the path, it will automatically call node_load() and the page callback apps_view_node() receive a fully loaded node object.
/**
* Implementation of hook_menu.
*/
function apps_menu() {
  $items = array();
  // With this menu callback, apps_view_node() will receive a node object, instead of an integer.
  $items['apps/%node/view'] = array(
    'type'           => MENU_CALLBACK,
    'page callback'  => 'apps_view_node_obj',
    // 1 is the node object, 2 is 'view'.
    'page arguments' => array(1, 2),
    // Tells the load callback function, node_load(), what part of the URL to load, in this case the literal number 1.
    'load arguments' => array(1),
  );

  // With this menu callback, apps_view_node() will receive an integer.
  $items['apps/%/edit'] = array(
    'type'           => MENU_CALLBACK,
    'page callback'  => 'apps_view_node_int',
    'page arguments' => array(1),
  );
  return $items;
}

/**
* Custom node view function.
* @param StdClass $node
*   Fully loaded Drupal node object.
*/
function apps_view_node_obj($node) {
  // Do something with the $node object.
  $node->title = "Foo";
  $node->body = "Bar";
  node_save($node);
}

/**
* Custom node view function.
* @param int $id
*   Node id.
*/
function apps_view_node_int($id) {
  // Because we are receiving an id, we must manually load the node object.
  $node = node_load($id);
  $node->title = "Hello";
  $node->body = "World";
  node_save($node);
}

Link to hook_menu documentation.

redpajama_set_name: RedPajamaStackExchange


Kolamavu Kokila (lit. Kolam-powder Kokila) is a 2018 Indian Tamil-language black comedy film, written and directed by Nelson Dilipkumar and produced by Lyca Productions. The film stars Nayanthara in the lead role alongside Yogi Babu and Saranya Ponvannan with Jacqueline playing key role. Anirudh Ravichander composes the film's live music. This film received highly positive response.
Kokila is an ordinary girl who gets into the business of drugs due to her family circumstances and her mother's illness. How she tackles and comes from the situation forms the crux of the story .
Ranbir Kapoor and Alia Bhatt: Candid pictures of the duo you shouldn't miss!
Is Nayantara Planning For A Secret Marriage…?
Nayanthara To Play Anushka Sharma's Role In Pari Remake?
U-Turn revamp: Narain lands a key part in Samantha Akkineni starrer !!


Fly Worry Free is a full-service travel agency that can quickly and professionally handle all your travel needs. With over 30 years of combined industry experience, we have the knowledge and resources to deliver quality airline tickets, rental cars, and tour packages for the lowest prices on the market.
We offer the ease and convenience of online ticketing, perfect for quick trips with simple itineraries. You can book a flight and reserve a rental car with just a few clicks. Our industry-leading booking engine will seek out the absolute lowest fares available online.
For more complex itineraries, or to book one of our all-inclusive tour or resort packages, we give you the option of speaking directly with an experienced Travel Professional. Even the best online retailers can offer only a handful of options. But our Travel Professionals use industry-leading tools and resources to help you customize every single aspect of your trip. You can choose your favorite airline and make special requests for meals and services . You can personalize hotel accommodations, and even learn how to make the most of your layover when travelling internationally.
Our Travel Professionals also save you money when booking last minute flights, especially in first- and business-class. Working under exclusive agreements with airlines and ticket consolidators, we can offer last minute bookings for corporate fliers at hundreds less than you'll find anywhere online.
We'll also be on-call 24/7 as an exclusive service for our corporate clients. You'll have a direct line to a dedicated travel manager who will answer urgent inquiries and make last minute changes at any time, day or night.
So whether you're looking for the ease and convenience of online service, or the personal attention of a friendly and knowledgeable agent, Fly Worry Free offers you the best service at an unbelievable value. Book with us today and let us help you Fly Worry Free.


The Mail Merge fields feature allows you to personalize your Email campaign with Lead Details, Sender Details and also company details, without having to manually write the information in the Email. Mail Merge fields allows you to personalize the Sender Name, Subject Line, HTML message, Email footer and also the Text message. By using this feature, each lead or recipient receives a personalized Email.
The custom fields that are present in your LeadSquared account can be used as Mail Merge fields. For instance, Lead First Name, Company and so on.
Visual Designer – This is a drag-drop editor which allows to create responsive design Emails.
Rich-Text Editor – Allows you to add formatting and pictures to text without using HTML tags.
Plain Text Editor – Allows you to create simple plain-text email with no images or text formatting.
HTML Editor – Allows you to change the look and feel of your Email content using HTML markup.
How to Insert Mail Merge Tags for the Subject Line and Email Body?
From the right-hand side of your Rich Text/Plain Text/HTML Email Editor, under Email Personalization, select the required category of Mail Merge tags from the drop-down field.
Place your cursor on the subject line of the Email and click the required Mail Merge field. The Mail Merge field is added to the subject line.
Select the required Mail Merge category under Email Personalization.
Place the cursor in the required position in the Email body and click the required Mail Merge field to add.
Note: You can add multiple Mail Merge fields to your Subject line or Email body.
From the Visual Designer Email Editor window, place the cursor on the required text area of the Email body. A tool bar appears.
Click Merge tags from the tool bar. The Insert Merge tags pop-up box appears.
Click the required Mail Merge tag and it is added to the Email body.
Note: To add Mail Merge tags to the subject line of the Visual Designer, copy/paste the Mail Merge tags to the subject line after adding to the Email body.
If you want to use a particular Mail Merge field which is not present in your LeadSquared account, you can create a custom field and include that in the Mail Merge box. For more information, see How To Create Custom Fields?


text:
Andrew McCabe reportedly has memos detailing his interactions with Trump. Here is everything we know.
Chris Enloe
Andrew McCabe reportedly kept memos detailing his interactions with President Donald Trump, just like his former boss, former FBI Director James Comey. (Alex Wong/Getty Images)
Former Deputy FBI Director Andrew McCabe, who was fired on Friday, kept memos detailing his conversations with President Donald Trump, the Associated Press reported Saturday.
BREAKING: AP learns fired FBI deputy director Andrew McCabe maintained personal memos regarding President Donald Trump.
— The Associated Press (@The Associated Press) 1521306046.0
McCabe's former boss, James Comey — who was FBI Director before Trump fired him last May — also kept memos on his conversations with Trump, which became a large story last year in the fallout of Comey's dismissal and his decision to leak information to a close lawyer friend.
An anonymous source "with direct knowledge of the situation who wasn't authorized to discuss the memos publicly" told the AP McCabe's memos are very similar to those that Comey kept. The memos reportedly contain information about McCabe's interactions with Trump, "among other topics."
As the AP noted, it's unclear if special counsel Robert Mueller has requested or reviewed the memos. He did review Comey's memos last year.
McCabe has already said he believes his termination, which came just days before his planned retirement, was an "attack" on his "credibility," and is "a larger effort not just to slander me personally, but to taint the FBI, law enforcement, and intelligence professionals more generally."
"It is part of this Administration's ongoing war on the FBI and the efforts of the Special Counsel investigation, which continue to this day. Their persistence in this campaign only highlights the importance of the Special Counsel's work," McCabe said in a statement.
McCabe has already lawyered up, according to the Daily Beast.
Update: The Wall Street Journal reported Saturday afternoon that McCabe has turned over his memos to Mueller. CNN later confirmed the Journal's report.
The Federal Reserve moves forward with digital currency initiative


Let your tastebuds rejoice with this mix of vanilla and fleur de sel. Ideal with fish and shellfish, this mix will enchant duck and sweet and sour dishes.
This mix of fleur de sel and vanilla from Madagascaris ideal with chocolate desserts. The floral aromas and scents of vanilla and subtle aromatic notes of anise and exotic fruits are delicious with creamy dishes. You can also add it to shortcrust pastry, scallop carpaccio, squash soup or gougere cheese puffs.
The crystals of fleur de sel are finer than those of traditional sea salt. The fine light texture means it dissolves quicker and blends more easily with all your dishes. Fleur de sel benefits from the expertise of the Malagasy salt workers and an ideal coastal climate. A thin crust of white crystals forms on the surface of the salt ponds when the water evaporates due to the sun and the wind.


text:
ARCHIE Collection
ARCHIE Collection(2016-2018)
Genres: Kids & Family, Adventure
A.R.C.H.I.E. 2: Mission Impawsible(2018)
1h 22min | Kids & Family, Adventure
2.8/5 (with 1 vote)
In this sequel, the super intelligent artificial robotronic dog, Archie, befriends Gregory, a young boy who is the son of a carnival owner. Gregory is concerned that someone has been stealing from the carnival and enlists his new friend to help find the culprit.
Rent Amazon Instant Video | Buy Amazon Instant Video
A.R.C.H.I.E.(2016)
1h 28min | Kids & Family
A recently orphaned 15-year-old who has moved to a small town to live with her uncle befriends a robotic canine with super strength, x-ray vision and the ability to talk and the pair take on a military complex, bullies, kidnappers, romance and the world.
Directed by Robin Dunne
WatchPlayStream is your search engine for movies and series streams/downloads. Always get the best overview of new movies on Amazon Prime Video, Netflix, iTunes Store and other providers. Where can you find the best TV shows & series for free streaming? Who offers movies and series like No Sudden Move, There's Someone Inside Your House, West Side Story, Resident Evil, The Purge and Mickey Mouse Funhouse for legal download? What haven't you seen yet? WatchPlayStream has the answers! Create a free account to manage your movies/TV series.


text:
Dark Souls 3 IGT, autosplitter and nologo for [LiveSplit](https://github.com/LiveSplit/LiveSplit/)

IGT by [Jiiks](https://github.com/Jiiks)

Autosplitter by [B3LYP](https://github.com/pawREP)

No Logo Mod by [blcd](https://github.com/bladecoding)

redpajama_set_name: RedPajamaGithub


Autumn days traditionally mean that bright lipsticks tend to be and opt for warmer, more muted shades. This Autumn/Winter is no different however a few curve balls were in amongst the conventional shades on the catwalks this season.
On International Kissing Day or World Kiss Day (yes its a thing) I posted an Instagram picture of my lips which got a lot of love on both my accounts (@organicmua / @eyeslikepandas) and so I felt I should share it with you on here too.
The newest kid on the lip colour block is liquid Lipstick. In short a these tubes of colour have all the pigment you'd expect of a traditional bullet style lippy but the texture and slip of a gloss and the staying power of a stain. They are quite literally liquid lipsticks.


All the talk about alligators and crocodiles reminded me of the FX series Archer episode Pipeline Fever (Season 2 episode 4 on Netflix). It takes place in the Louisiana bayou, and is pretty funny. Since you seem to have an affinity for gator related attacks I'd recommend checking it out the episode and series if you haven't already.
Good to hear Mom again, Paul! And for such a fine movie, too – I imagine she had a warm, nostalgic feeling sitting down with you and watching Yet Another Rubber-Suit Monster.
More M.O.M. and more Italian movies, please.
Great to hear M.O.M. again! I hope she has the time to start doing the podcast regularly again.
I had a small role in this film back then!
After making love on the Island! I just didn't make it to shore on time!!


Professor Kathleen Bell presented joint work Assistant Professor Caroline Noblet "Environmental change and recreation demand: Assessing interactions between beach width and beach recreation demand" at the W4133 (Costs and Benefits of Natural Resources on Public and Private Lands) Annual Meeting, in Santa Fe, New Mexico February 20-22, 2019. Bell and Noblet collaborated with Maine's Coastal Program to collect data at Popham Beach State Park. Bell and Noblet's ongoing research suggests beach users are responding to shoreline change at Popham Beach State Park in different ways and have different views about the preferred management response to such change.


text:
The Blind Boy
A blind boy sat on the steps of a building with a hat by his feet. He held up a sign which said: "I am blind, please help." There were only a few coins in the hat.
A busy man was walking by the building when he saw the boy. The man stopped, thinking for a moment. He took a few coins from his pocket and dropped them into the hat. He then took the sign, turned it around, and wrote some words on it. He put the sign back in such a way that everyone who walked by would be able to see the new words.
Soon the hat began to fill up quite quickly. A lot more people were giving money to the blind boy.
That afternoon the man who had changed the sign came to see how things were. The boy recognized his footsteps and asked, "Were you the one who changed my sign this morning? What did you write?"
The man said, "I only wrote the truth. I said what you said but in a different way."
What he had written was:
"Today is a beautiful day and I cannot see it."
Afterthought
Do you think the first sign and the second sign were saying the same thing?
Of course both signs told people that the boy was blind. But the first sign simply said the boy was blind. The second sign told people they were so blessed that they were not blind. Should we be surprised that the second sign was more effective?
"It is He, Who has created for you (the sense of) hearing (ears), sight (eyes), and hearts (understanding). Little thanks you give."
[Surah Al-Mu'minun; 78]


Items from the Pacific region gathered by Jane Stanford and faculty members are on display as part of a new exhibition at the Stanford Archaeology Center curated and installed by students under the instruction of Christina Hodge, academic curator and collections manager for archaeology collections.
The new Stanford exhibition, "From 'Curios' to Ambassadors: Changing Roles of the Daggett Collection from Tribes of the Lower Klamath River," highlights Native American tribal objects in a way that more precisely reflects their origins. It is on view through June 4, 2016.
The "City Beneath the City" installation at the Stanford Archaeology Center combines history and art for an insightful examination of local Bay Area history.


text:
November 20, 2020Events Music
Photo courtesy of Present Music
How Present Music Is Creatively Adapting Their Annual Thanksgiving Concert
A concert to Zoom into before you give thanks.
BY Marla Hiller
Present Music, a Milwaukee institution dedicated to contemporary classical music, is no stranger to unconventional venues. In 2011, for instance, ensemble members played instruments while floating down the Milwaukee River – for listeners gathered along its banks. So it's hardly surprising that they feel comfortable hosting their Thanksgiving concert, titled "Wherein Lies the Good," over the videoconferencing app Zoom.
One of the hallmarks of this annual event has always been audience participation via singing and friendship circles. And co-artistic directors Eric Segnitz and David Bloom are determined to keep that tradition alive, even with a wholly virtual audience. How? They've invited Mark Stewart, a musician and instrument builder, to lead a "private duet" with audience members.
All ticket holders will receive care packages before the concert, containing homemade instruments that Stewart fashioned from Popsicle sticks. And, according to Stewart, when would-be music makers bite down on the stick and strum their fingers along its side, the reverberation will create subtle buzzing sounds that only they'll be able to hear. Hence, the "private" part of the "duet."
Ultimately the ensemble members and their collaborators – including the Reagan High School Choir and the Bucks Native American Singing and Drumming Group – hope to bring a little more togetherness to socially distanced city dwellers.
Present Music's 26th annual Thanksgiving concert will take place on Nov. 22, the Sunday before Thanksgiving. Tickets are available online at presentmusic.org.
This story is part of Milwaukee Magazine's November issue.
present music
5 Things to Do in Milwaukee This Weekend: Nov. 20-22
Your Official Black Friday Beer Guide
Marla Hiller
Marla Hiller is an editorial intern at Milwaukee Magazine. She is a junior at Boston University majoring in international relations and minoring in journalism
10 Things to Do in Milwaukee This Weekend: Jan. 27-29
How DanDan Is Celebrating the Lunar New Year


Actor? Director? Producer? Your call - but you can do them all at the Studio!
The Career home for the Actor, your Sim will work between the hours of 9:00 AM and 5:00 PM.
The Camera is the tool you can obtain from The Hobby Shop to train this skill at home.
If it says it will take over 300 hours than you have used the time skip cheat. That is one of the bad side-effects of that cheat and it is one reason why we suggest NEVER to use that cheat. Ever. Your only option is to allow the timer to run out, with any luck that will unstick your game.
Ok guys, you go to the little store that sells the soccer ball and stuff like that, you then scroll across and as you scroll you should go past a movie camera for approximately 2,000 simoleons you purchase that. Then that should give you a head start. It's now up to you guys to finish! I really do hope I helped you and good luck!
I've started building my movie studio and it's saying it's going to take over 300 hours. Is this a glitch? How do I solve this problem?
how to cancel Movie Studio? please help me.
How do I use this to practice film making to pass level 9. Or add someone who has the camera. Help.
I downlod the Movie studio and i cant cancel it .How do i cancel it ?


text:
Kim Richards THROWS DOWN With Natalie Nunn on New Reality Show!
by Tyler Johnson at March 7, 2016 5:10 pm .
It's been almost two weeks since Kim Richards was involved in any sort of ridiculous drama, so you had to know something crazy was coming.
Last time we checked in on the troubled reality star, she was facing jail time after lying to a judge to get out of doing community service.
That matter won't be settled until Kim heads back to court on June 1, but in the meantime, she's bringing the crazy on her new Lifetime reality show, The Mother/Daughter Experiment.
In a clip from this week's episode, Kim gets into it with former Bad Girls Club Natalie Nunn, who's apparently sick of being called a "bad girl, " even though that's literally all she's famous for.
Note to other people who might try to be shedding their troublemaker reputation - getting into physical altercations while camera crews are present is generally not the best way to go about it.
On the bright side, the clip supports claims that Kim is sober now, and she's actually serving as the voice of reason for once.
Yes, when you're Kim Richards, taking of your sweater so that you can throw down with a woman who's carrying a plate of Totino's pizza rolls is actually a sign of progress. Baby steps.
Kim Richards Videos, Celebrity Gossip Videos
Kyle Richards: BEGGING Sister Kim Richards to Seek Treatment
Kim Richards: Returning To RHOBH As A Full-Time Cast Member?!
The Real Housewives of Beverly Hills Recap: BunnyGate Returns!
Kim Richards Photos
Kim Richards Videos
The Real Housewives of Beverly Hills Finale Clip: Look Who's Back!
The Real Housewives of Beverly Hills Clip: Kim vs. Kyle!


text:
No One Said Climbing Wasn't Hard
Vol 12, Issue 4
JANELLE KOH
When you got your mid-semester marks back, they were much lower than you expected. Lower than you would ever have expected of yourself. The people around you did better than you, and you're happy for them, but can't shake the feeling that you're better than this. (You are.) You think about the circumstances surrounding the assignments. Something had been going wrong for a while. A panic attack had hit you, early this semester. It shakes your hands still, now and again, like an old friend whose face looks different from how you remembered. But you tell yourself you can't blame the marks on that alone. You say you could've worked harder, smarter. But you won't tell yourself you should have.
You know when you say 'should have', you mean that there are more valuable outcomes than the one you got. You could've gotten a better mark, probably. Could've felt better about yourself, about the whole damn thing. But the only real thing you get out of doing better, the only really real thing, is not having to deal with the way we treat marks like they're wounds. And is that all that desirable?
In her poem 'climbers', Ellen van Neerven restates the above. She writes: "the hold patterns in the bunya pine...do not fit hands/ or feet anymore/but it is not a wrecked kind of meaning...marks are not wounds." Though the 'marks' Ellen speaks of aren't grades, the truth of her words still apply. You couldn't hold on to as many marks as you would've liked. They didn't fit you this time, for whatever reason - perhaps you were dodging branches at the time. But those marks are not for you to take on, to ingest and allow to become your wounds, to wreck your meanings. But if marks are not wounds, and they don't look like holds... what are they?
You remember going rock climbing in the gym the other day, as a beginner. You remember seeing that as the difficulty of the climbs got harder, the holds barely imprint on the rock. These holds didn't look much like holds at all, but they were called 'holds' for a reason. They held meaning, one that you perhaps didn't have the techniques with which to understand. You didn't know how to scramble up walls; to use your momentum; when to stand instead or crouch, or when to crouch instead of stand. But on one climb you were already halfway up the wall. You weren't about to let yourself down. You knew only how to jump and put one hand in front of the other, so that's what you did. You jumped and grabbed, your hand slipped and you fell, but the harness caught. You swung slowly in mid-air. You felt a little like a fairy in a school play, and realised then that this was all pretend. If you don't grasp these plastic handholds, all it means is you didn't grasp it, and therefore you should try again. There's no use denying that hold had meaning. Trust yourself, and know that you wouldn't have begun to climb the wall, wouldn't have gotten this far up unless it meant something to you to do it. Know that you're not going to get hurt, unless you let yourself. Unless you're negligent, unless you beat yourself up about it, unless you get angry and kick something you shouldn't. You've done all those things. You know not to do them anymore. Let yourself dangle with grace, and remember that you're swinging, not falling. Is that all a law school grade is, a plastic handhold? Is that all this brand of failure represents? I think so. (That's as close as I can get to understanding it today, anyway.)
So don't worry if you're not brilliant in the ways those tests need you to be. Don't worry about the 62%, the 57%, or how others seem to be going better than you. There are so many things you're dodging, some of which you maybe don't realise - though trust me, they are real. But don't forget about the marks altogether. See them for what they are: things to learn from, things that are there to help you be better - things to hold on to.
Marks are not wounds. Marks are not wounds. Marks are not wounds.
Janelle Koh is a second-year JD student
Not Everything Has to Make Sense
We'll all be dead a century from now. What's the difference between a 65 and an 80 when you're rotting underground?


If you are interested in being in the 2016 Collier County Fair, Click here to get the Concession Application, Fire Department Rules and Health Department Information. Complete the forms and Fax them back to (239) 455-6701 or Email them back to concessions@colliercountyfair.com or Mail it back to the Fair Office to the address on the application.
The Red Roof Inn Plus and Suites by Clicking here or call (239) 774-3117.


Secretive brothers own almost 16% of retailer Metro.
Secretive brothers own almost 16% of retailer Metro. Also own Travel Charm, a chain of 12 luxury hotels and spas located in Germany, Austria and Italy. Fund the Mercator Foundation which helps immigrant children in Germany improve their language and professional skills through extracurricular study programs.


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Places to Go > State Parks > Iowa State Parks > Green Valley State Park
Green Valley State Park in southwest Iowa is a popular destination for fishing and boating. The park is a family-friendly hub for camping, picnicking or any outdoor pursuit. Four lakes in the region -- Three Mile Lake, Twelve Mile Lake, Summit Lake and Green Valley Lake -- are located within 10 miles of each other and create a hub for lake recreation in southwest Iowa.
Hike almost 10 miles of trails at Green Valley, winding through wetland areas around the fringes of the lake to woodlands and remnants of native prairie. Mountain biking is an option on the trails, which are a combination of pavement and roadways.
Fish for walleye, bluegill, channel catfish and more at Green Valley Lake. Two ADA accessible fishing piers are available on the north and south shorelines.
Boat in the waters of Green Valley Lake or swim at the sandy beach area. Boats must operate at "no-wake" speeds and cannot be operated at more than 5 mph within 100 feet of the shore or within 50 feet of another craft or person. In-board motors are not allowed on the lake, including jet skis and jet boats. Water skiing is allowed in a designated area and all water skiers must wear a U.S. Coast Guard approved life-jacket.
Stay overnight in one of three camping cabins or at the park's campground. Camping cabins include a covered porch, electricity, a microwave and small refrigerator but do not have water or sanitary facilities. The campground offers electric and full hook-up sites, modern restrooms and showers and a trailer dump station. One-fourth of the campsites are available on a first-come, first-served basis and advance campsites reservations can be made online through the online reservation system for Green Valley State Park.
*High Lake Outdoor Alliance offers firewood sales to campers and from April 1 to October 31 when the campground host is available.
Reserve one of two open shelters for an outdoor gathering during your visit. Scenic picnic areas can be found throughout the park and the shelter can be reserved through the online reservation system for Green Valley State Park.
Green_Valley@dnr.iowa.gov
Park Map and Flyer [PDF] Green Valley Campground Map [PDF] Green Valley Trails Map [PDF] Special Deer Hunt Information [PDF] Volunteer Opportunities Beach Monitoring Information Iowa State Park List
Boat ramps (4)
Universally accessible fishing piers (2)
Fishing jetty
Fish cleaning station
Modern restroom
Camping cabins (3)
Buddy campsites (6)
Group campsites (2)
Electric campsites (48)
Full hook-up campsites (15)
Tent only campsites (17)
Youth group only campsites (1)
Trailer dump station
Firewood sales


text:
"Take Me with U" is a song by Prince and the Revolution, and the final US single released from their album, Purple Rain (1984).

Background
The song is sung as a duet with Apollonia Kotero, and was originally intended to be performed by Vanity but shortly before filming began on the movie Purple Rain, Vanity famously chose to quit participation in the film altogether when she was offered what appeared to be a lucrative contract with Motown Records exec Berry Gordy and began filming The Last Dragon (An early demo of the song exists with her vocals and has circulated on bootleg recordings by collectors.) and ceased her romantic relationship with Prince. The song was then intended for the Apollonia 6 album to coincide with the film, but was pulled for the Purple Rain soundtrack. A result of this addition, Prince made cuts to the suite-like original "Computer Blue", which circulates among collectors in an extended version (a portion of this second section of "Computer Blue" can be heard in the film Purple Rain as Prince walks in on the men of The Revolution rehearsing). The original version of the song was about a minute longer.

Reception
Cash Box said that the song has "some beautiful melodies and some well-placed string sections which are proof of Prince's varied talents."

Chart performance
The single was released with an edit of album track "Baby I'm a Star" as its B-side. In the US, it reached number 40 on the Hot Black Singles chart and reached number 25 on the top 40 chart. In the UK, the song was issued as a double A-side single, coupled with "Let's Go Crazy", reaching number 7 in February 1985.

Personnel
Credits are adapted from Prince Vault and the album's Liner Notes
 Prince – lead vocals, guitars, overdubbed tom-toms, string arrangement
 Apollonia – co-lead vocals
 Wendy Melvoin – string conductor, guitars, background vocals
 Lisa Coleman – string arrangement, string conductor, keyboards, background vocals
 Matt Fink – keyboards, background vocals
 Brown Mark – bass guitar, background vocals
 Bobby Z. – drums, percussion
 David Coleman – cello
 Suzie Katayama – cello
 Novi Novog – violin and viola

Track listing

7": Paisley Park / 7-29079 (US)
 "Take Me with U" (edit) – 3:42
 "Baby I'm a Star" (edit) – 2:55

References

1984 songs
1985 singles
Prince (musician) songs
Songs written by Prince (musician)
Male–female vocal duets
Warner Records singles
Song recordings produced by Prince (musician)
American psychedelic rock songs
Songs written for films

redpajama_set_name: RedPajamaWikipedia


text:
Dioctria oelandica är en tvåvingeart som först beskrevs av Carl von Linné 1758.  Dioctria oelandica ingår i släktet Dioctria och familjen rovflugor. Arten är reproducerande i Sverige. Inga underarter finns listade i Catalogue of Life.

Källor

Rovflugor
oelandica


I'm so excited for this event ! S/S13 with Harvey Nichols ! There is a demand for tickets so this year the event is taking place in the Old Post office at the Mailbox, where last years Style Birmingham was held and the show is expected to attract over 400 guests !
The show has gained an amazing reputation and it's become the place to be for the fashionistas calendar with collections from Dolce & Gabbana, Gucci, Roberto Cavalli and Christian Louboutin.
If you want to be one of those 400 then head on over to www.theticketfactory.com/harveynichols or call 01216166008. Tickets are £15 and the evening kicks off with a Champagne reception at 7pm and then after the show enjoy 15% off in store.


Stockholm-born, Cape Town-based and Michaelis School of Fine Art-graduate, artist Tom Cullberg shares his exciting upcoming local and international exhibitions, what he's reading at the moment, and who we should all be following on Instagram.
My current work is an amalgamation of the different styles I have explored over the course of my career, from early figurative paintings composed of narratives of people and places, to striped paintings, book portraits and abstract works.
How much has the South African context influenced your work?
Coming from Sweden to South Africa in the '90s, I was met with a very different society from what I was used to, but also a radically changing society with many contrasts. With my work I try to make sense of these impressions and identify places of connection, communication and belonging; foster an awareness of history, both private and public. There is a play between these dualities: the insider and the outsider, the notion of home, the past and the present.
I am happy where I live now in Cape Town, but if I could, I would like to spend some time in Japan.
My new solo show Finding New Life in an Old Form opens at Barnard on 21 August 2018. I'm busy with final preparations for that as well as finishing off paintings that will be presented by Barnard at START Art Fair in London, which takes place at the Saatchi Gallery from 13 to 16 September 2018. I'm also in the planning stages for paintings that will be included in Barnard's forthcoming presentation at Also Known as Africa (AKAA), the first art fair devoted to contemporary art and design from Africa to be organised in Paris from 9 to 11 November 2018.
My kids, friends, music, books and films, architecture and furniture design, cities, memories/ remembering and perhaps most importantly the act of painting in itself.
Describe where you create your pieces/your studio?
My studio is located at the Side Street Studios in Woodstock. It's a calm space, usually quite neat and fairly ordered. I have geraniums growing in the windows and quite a lot of books. A daybed is my favourite spot for looking at the work and contemplating my next moves. A few of my artist friends work nearby and it's great to break the solitude with a coffee or a chat.
I like the late afternoon. I start painting in the morning, but I find painting takes a lot of warming up time. By the afternoon I have usually found my pace.
Tom Cullberg in his studio in Cape Town.
I'm "reading" Haruki Murakami's Dance Dance Dance and Donna Tartt The Secret History – one is an audiobook and the other paperback.
I can't imagine being anything else!
Aside from @visi_mag, who should we all be following on Instagram?
Artists Jules de Balincourt, Sara-Vide Ericson, Cameron Platter and Tom Sachs, Bill Powers of Halfgallery, and The New Yorker.
Follow Tom on Instagram and catch his latest exhibition, Finding New Life in an Old Form, from 21 August until 2 October 2018 at Barnard, 55 Main Street, Newlands, Cape Town.


text:
package apollo.dataadapter.ensj.controller;

import apollo.dataadapter.ensj.*;
import apollo.dataadapter.ensj.model.*;
import apollo.dataadapter.ensj.view.*;
import java.sql.*;
import java.util.*;

/**
 * Check to see if our gene counts have already been initialised. If not,
 * run sql to get them. Populate the table of gene types, gene counts (by type)
 * and set the 'gene counts by type initialised' flag to true. Tell the gui
 * to display the gene types list.
**/
public class ShowGeneCountsByTypeHandler extends EventHandler{

  public ShowGeneCountsByTypeHandler(Controller controller, String key) {
    super(controller, key);
  }

  public void doAction(Model model){
    TypesModel myModel = model.getTypesModel();
    HashMap geneTypeCounts;
    log("Fetching & showing gene counts by type");

    doUpdate();

    if(myModel.getTypePanelToShow().equals(myModel.GENE)){
      log("Setting NO type panel to show (hiding gene type panel)");
      myModel.setTypePanelToShow(myModel.NONE);
    }else{
      log("Setting type panel to show type "+myModel.GENE);
      myModel.setTypePanelToShow(myModel.GENE);
    }

    if(!myModel.isGeneTypeCountInitialised()){
      log("Initialising gene type count");
      geneTypeCounts = getGeneCountsByType(model);
      myModel.setGeneTypeCounts(geneTypeCounts);
      ArrayList geneTypes = new ArrayList(geneTypeCounts.keySet());
      Collections.sort(geneTypes);
      myModel.setGeneTypes(geneTypes);
      myModel.setGeneTypeCountInitialised(true);
    }

    doRead();
  }

  public HashMap getGeneCountsByType(Model model){
    HashMap returnMap = new HashMap();
    Connection connection = getConnectionForModel(model);
    //String sql =
    // "select logic_name, count(*) from gene, analysis where gene.analysis_id = analysis.analysis_id "+
    // "group by gene.analysis_id";

    // This code is a bit hacky at the moment because its trying to cope with the transition from schema 20+ to schema 32+ where the
    // gene table columns changed
    int schema = EnsJConnectionUtil.getEnsemblSchema(connection);

    String sql;
    if (schema > 32) {
      sql = "select biotype,count(*),status,source from gene group by biotype,source,status order by biotype,source,status";
    } else if (schema == 32) {
      sql = "select biotype,count(*),confidence,source from gene group by biotype,source,confidence order by biotype,source,confidence";
    } else {
      sql = "select type,count(*) from gene group by type order by type";
    }

    ResultSet results;

    try{

      results = connection.createStatement().executeQuery(sql);
      while(results.next()){
        String typeStr;

        if (schema > 30) {
          typeStr = (results.getString(1) == null ? "" : results.getString(1)) + "_" +
                    (results.getString(3) == null ? "" : results.getString(3)) + "_" +
                    (results.getString(4) == null ? "" : results.getString(4));

        } else {
          typeStr = results.getString(1);
        }

        //System.out.println("Type string = " + typeStr);
        returnMap.put(typeStr, new Integer(results.getInt(2)));
      }

      log("Found "+returnMap.keySet().size()+" Different types");
      connection.close();
    }catch(SQLException exception){
      throw new NonFatalException(exception.getMessage(), exception);
    }

    return returnMap;
  }

}


Here are some photos from the set/facebook pages of Dino Lee and Esther Wu as they start filming! I think the drama is slated to be out sometime in December, although I haven't found a hard date yet. I'm also not too sure if I'll watch it, mainly because I feel like I've outgrown the dumb girl smart cold guy trope and it gets a bit tiring with each remake (also, the Kdrama just flat out had no chemistry. so there's that).
You guys copied most everything like in playful kiss.
Actually, Playful Kiss is also a remake (licensed from the manga writer).The original story if you're interested is a manga called Itazura na Kiss.