text:
\section{Introduction}

All galaxies are thought to undergo active phases where the central supermassive black hole (SMBH) accretes galactic material. Active Galactic Nuclei (AGN) are believed to play a role in regulating star formation and transforming blue, star forming galaxies into red, passive galaxies \citep[e.g.][]{hopkins08,hickox09}.
Evidence also points to a co-evolution of supermassive black hole mass and host galaxy properties such as bulge mass and velocity dispersion \citep[e.g.][]{magorrian98, silk98}, implying a connection between the evolution of the galaxy and AGN.

AGN fueling is dependent on both the gas supply available to a galaxy, and the efficiency with which that gas can be deposited on the central SMBH.  The former is influenced by the large-scale environment in which a galaxy resides, while the latter depends upon whether mergers \citep[e.g.,][]{hopkins08} or secular processes such as  bar instabilities and galaxy interactions \citep[e.g.,][]{goulding14} are the dominant mechanisms for triggering AGN. The dense, rich environment of galaxy clusters, with high densities of galaxies and intracluster material, provides a unique regime in which to study the impact of large-scale environmental factors. In the outer regions of galaxy clusters, the cluster environment can increase merger rates and the frequency of tidal perturbations as compared to the field, triggering AGN. Meanwhile, in the cluster cores, the intracluster medium (ICM) can quench galactic star formation and AGN fueling by removing the fuel supply. The ICM can unbind gas from the halos of infalling galaxies \citep[strangulation;][]{larson80}, while leaving the cold central gas intact, stifling the galaxy's ability to accrete new cold gas after depleting its initial cold gas content. It can also remove cooler gas within the galaxy via ram pressure stripping \citep{gunn72}.
However, the relative importance of different AGN triggering mechanisms, including major and minor mergers and secular processes such as bar instabilities and galaxy interactions, remains an open question.

Conversely, the AGN can also impact the galaxy cluster environment. Radio-mode feedback plays an important role in regulating the cooling of hot gas from the ICM and limiting star formation. The feedback scenario is used to explain the lack of star formation in the inner cluster galaxies. In radio-mode, the energy from the AGN is deposited in the ICM by radio-emitting jets, creating low-density bubbles \citep[e.g.][]{peterson03,fabian12}. Observations of the X-ray cavities in clusters, formed by the transfer of mechanical energy into the ICM, suggest that AGN regulate cluster cooling at redshift $z\sim1$ during major assembly of the cluster and ICM \citep{hlavacek-larrondo15,mcdonald15}.

The literature on the frequency of AGN in galaxy clusters is mixed on how the environment impacts AGN triggering. The measured cluster AGN content can depend on factors such as the redshift, mass, and AGN selection method used in the study. Early work showed AGN are less likely to reside in galaxy cluster environments at $z\sim0.04$ \citep{dressler85}. However, more recent studies have shown the number of AGN in clusters and the ratio of AGN to cluster galaxies increases with higher redshift \citep{galametz09,martini09,martini13,pentericci13,bufanda17}.

Early surveys also relied on optical spectroscopy, which is insensitive to obscured, Compton-thick AGN. With the addition of multi-frequency AGN surveys, a more nuanced picture of AGN in galaxy clusters emerges. Mid-infrared (MIR) selection has the benefit of being able to detect AGN obscured by dust. Ultraviolet light reprocessed by the dusty torus is bright in MIR bands but would otherwise be missed by optical selection \citep[e.g.,][]{lacy04, stern12, donley12}. Selection by radio and X-ray emission stemming from the AGN's nuclear activity is also advantageous in that sources that emit strongly in these wavelengths are very likely to be AGN. \citet{galametz09}, using AGN catalogs selected in the radio, infrared, and X-ray, report an increase in the amplitude of overdensity of AGN in clusters as a function of increasing redshift. \citet{croft07} estimate that $20\%$ of all low-redshift galaxy clusters have a radio-detected brightest cluster galaxy (BCG). Multiple studies using X-ray data show an excess of AGN in the central regions of galaxy clusters \citep[e.g.][]{ebeling01, ruderman05, ehlert13}.

Detailed observations reveal variations in the number of cluster AGN as a function of clustercentric distance. \citet{pimbblet13}, studying six galaxy clusters at $z\sim0.06$, find that the fraction of spectroscopically-confirmed optically-selected AGN increases from cluster center to $\sim2r_\mathrm{virial}$, beyond which the AGN fraction declines. In $42$ clusters at $0.2<z<0.7$, \citet{ehlert14} calculate an X-ray AGN fraction that is $\sim1.5-3$ times lower than the expected AGN fraction in the field in the innermost $\sim{r_{500}}$ and converges to expected field values beyond $\sim2r_{500}$.  \citet{haines12} find that the X-ray selected AGN population in a sample of 28 massive clusters at $0.15<z<0.30$ are dynamically associated with an infalling population and are preferentially aligned with the cluster caustics, and shows the efficacy of the cluster environment at suppressing nuclear activity in cluster members. Several authors also find tentative evidence for a secondary peak of AGN near the virial radius of the galaxy cluster \citep{ruderman05,fassbender12,koulouridis14}, which they attribute to an enhancement of the merger fraction in the cluster infall region. \citet{ehlert13} find weak evidence for a secondary excess between $1.5-2 r_{500}$ in all X-ray bands for the X-ray source radial profile in $43$ ROSAT All Sky Survey galaxy clusters, but did not find higher rates of AGN triggering near the virial radius as compared to the field when their sample was expanded to $135$ clusters \citep{ehlert15}. \citet{fassbender12} suggest that the secondary excess could be a function of cluster mass, where more massive galaxy clusters have a higher velocity dispersion that is less conducive to galaxy mergers.

We are motivated to revisit the study of AGN in galaxy clusters with a much larger cluster sample at high redshift. This paper presents a study of AGN at the positions of 2300 galaxy clusters at $z\sim1$ discovered with the Massive and Distant Clusters of WISE (MaDCoWS) survey. Section~\ref{sec:data} introduces the MaDCoWS data along with the AGN catalogs. We discuss the methods and results of the distribution of cluster AGN overdensities and fractions in Sections~\ref{sec:agndist} and \ref{sec:agnfrac}. In Section~\ref{sec:cluprop}, we investigate the dependence of AGN on cluster mass and central radio activity. We discuss the implications of our work in Section~\ref{sec:discussion}.

Throughout the paper, we adopt the nine-year Wilkinson Microwave Anisotropy Probe (WMAP9) cosmology of $\Omega_\mathrm{M}=0.287$, $\Omega_{\Lambda}=0.713$, and $H_0 = 69.32$~km~s$^{-1}$~Mpc$^{-1}$ \citep{hinshaw13}. We convert angular distances to physical distances assuming $z=1$. Unless otherwise stated, all magnitudes are in the Vega system.

\section{Data}
\label{sec:data}

\begin{deluxetable}{lcccc}
\tabletypesize{\footnotesize}
\tablecolumns{5}
\tablecaption{Number of Galaxy Clusters within AGN Catalog Footprints\label{tab:clusters}}
\tablehead{\colhead{Cluster Sample}&\colhead{R09}&\colhead{A18} & \colhead{A18$\times$PS} & \colhead{FIRST}}
\startdata
MaDCoWS & 1063 & 1778 & 1703 & 1132 \\
~Spitzer Follow-up & 717 & 1217 & 1166 & 759 \\
~~$15\leq\lambda_{15}<22$ & 141 & 231 & 221 & 154 \\
~~$22\leq\lambda_{15}<40$ & 449 & 758 & 727 & 483 \\
~~$\lambda_{15}\geq40$ & 127 & 228 & 218 & 122 \\
Radio-Inactive & 747 & 920 & 920 & 920 \\
Radio-Active & 172 & 212 & 212 & 212

\enddata
\end{deluxetable}

\subsection{Galaxy Cluster Sample}
\label{sec:clusample}

MaDCoWS \citep{gettings12,stanford14,brodwin15} identifies galaxy clusters as infrared-selected galaxy overdensities using the {\it Wide-field Infrared Survey Explorer} \citep[{\it WISE},][]{wright10}. Using the combination of {\it WISE} and Panoramic Survey Telescope and Rapid Response System \citep[Pan-STARRS,][]{kaiser02} data, MaDCoWS covers $17,668$~deg$^{2}$. At $z\sim1$, MaDCoWS provides the largest galaxy cluster sample at this epoch. For survey specifics, we refer the reader to \citet{gonzalez18}. In our analysis we use the $2300$ most significant MaDCoWS cluster candidates and refer to this sample as the ``MaDCoWS Cluster Catalog." For all clusters we use the WISE positions derived during the cluster detection process.

This project also relies upon {\it Spitzer} IRAC 3.6 and 4.5~$\mu$m snapshot observations of $1956$ cluster candidates obtained during Cycles 9, 11, and 12 (PIs: Gonzalez, Brodwin; PIDs 90177, 11080, 12101).  We refer to these clusters as the ``{\it Spitzer} Follow-up Clusters." Along with overdensity confirmation, the {\it Spitzer} data enables photometric redshifts and richness determinations, which are described in \citet{gonzalez18}. Briefly, photometric redshifts are derived using the combination of $i-[3.6]$ and $[3.6]-[4.5]$ colors of galaxies within 1$^\prime$ of the cluster location. The redshift is determined via a comparison of the peak of the galaxy distribution in color-color space with the predicted colors for a passively evolving galaxy formed via a single stellar burst at $z_f=3$.  The richness $\lambda_{15}$ is then defined as the number of galaxies with $[4.5]>15 \mu$Jy ($\sim5\times10^{10} M_\odot$ at $z=1$)
in excess of the field density that lie within 1 Mpc of the cluster center and have $i-[3.6]$ and $[3.6]-[4.5]$ colors consistent with being possible cluster members. Specifically, the galaxy must be no more than one magnitude bluer in $i-[3.6]$ than the peak color of the galaxy distribution, and must be within $\pm0.15$ mag in $[3.6]-[4.5]$. The {\it Spitzer} follow-up clusters range in richness from $\lambda_{15}=0.1-122$, though the interquartile range is from $\lambda_{15}=22-36$ ($M_{500}=1.0-2.6\times10^{14}~M_{\odot}$).

\subsection{AGN Catalogs}

We use literature catalogs of AGN selected by various methods. The number of galaxy clusters considered for the analysis in each subset will vary due to the different coverage area of each AGN catalog. These values are listed listed in Table~\ref{tab:clusters}.

\begin{figure}
    \centering
    \includegraphics[width=\columnwidth]{fig1}
    \caption{Spectra of two Type 1 and two Type 2 AGN candidates observed with Palomar DBSP on 22 November 2017. The Type 1 candidates were confirmed to be broad line AGN while the Type 2 AGN candidates are most likely narrow emission line galaxies.}
    \label{fig:spectra}
\end{figure}

\begin{figure}
    \centering
    \includegraphics[width=\columnwidth]{fig2}
    \caption{Overlap of sources in the AGN catalogs via optical-selection (R09), MIR-selection (A18) and radio signatures (FIRST) labeled by the number in each set.}
    \label{fig:catalogs}
\end{figure}

\subsubsection{Optical Selection}

\citet[][hereafter R09]{richards09} present a catalog of $1.2$ million quasars photometrically selected from the Sloan Digital Sky Survey (SDSS) Data Release 6. The catalog was constructed from SDSS point sources with extinction-corrected asinh magnitude $14.3<i<21.3$ (AB) from a 8417 deg$^{2}$ area.
R09 employ the Bayesian algorithm presented in \citet{richards04} to classify objects as quasars or stars based on a training set of $75,382$ quasars from published catalogs.

Using a method of auto-correlation of quasars presented in \citet{myers06}, R09 find a reliability of $71.5\pm3.5$\%. The completeness of the catalog to unobscured (Type 1) quasars is no worse than 70\%. A caveat is that the sample is relatively incomplete near $z\sim2.8$ and $z\sim3.5$, where the colors of stars and quasars are similar. It is also contaminated at $z\sim0.675$ by white dwarfs. R09 calculate an AGN catalog surface density of $141$~deg$^{-2}$. We refer to the R09 catalog as the ``optically-selected sample."

Though R09 also provides photometric redshifts for the catalog, accurate to ${\Delta}z=\pm0.3$ for 83\% of spectroscopically crossmatched sources, we choose not to select quasars based on redshift. In our analysis, we calculate the AGN field contribution by statistically subtracting foreground/background quasars. By not employing a photometric redshift cut, we also eliminate the possibility of selecting against quasars with miscalculated photometric redshifts.

\subsubsection{MIR Selection}

\citet[][hereafter A18]{assef18} have constructed a catalog using AllWISE data to photometrically select AGN via a two-color selection similar to that presented in \citet{assef13}. AllWISE is a combination of data from the {\it WISE} Full Cryogenic, 3-Band Cryogenic, and NEOWISE Post-Cryogenic survey. MIR selection distinguishes AGN from normal galaxies due to the infrared excess associated with AGN. In particular, MIR selection is less affected by dust extinction and can identify obscured, Compton-thick (Type 2) AGN missed by optical photometry.

We use the A18 $90\%$ reliability catalog, where $90\%$ of catalog objects are expected to be bona fide AGN, containing more than $4.5$ million sources. To reduce the non-uniformity due to the varying depth of the WISE survey strategy, we only consider sources with $W2<15.5$. This limit ensures all catalog sources are brighter than the AllWISE $95$\% completeness in W2 magnitude of $15.7$ and excludes fainter elliptical galaxies that may have colors consistent with an AGN\footnote{\url{http://wise2.ipac.caltech.edu/docs/release/allwise/}}. We also avoid catalog sources in the range $-30^{\circ}\leq\delta\leq-10^{\circ}$, a region with higher density due to the South Atlantic Anomaly. We refer to the $2,010,062$ MIR-selected AGN in the A18 catalog matching our criteria as the ``MIR-selected sample." The surface density of the catalog is $86$~deg$^{-2}$.

The full A18 R90 catalog is optimized for 90\% reliability at the expense of completeness. Comparing the R90 catalog to the AGN and Galaxy Evolution Survey \citep[AGES,][]{kochanek12} in the NOAO Deep Wide-Field Survey (NDWFS) Bo\"otes field, the R90 selection recovers 17\% of the NDWFS Bo\"otes AGN. Because we only consider brighter sources in W2, our completeness should be higher than that of the full R90 catalog, though calculating the completeness and reliability at the W2 limit we consider is beyond the scope of this paper. However, with a similar selection function as A18, \citet{assef13} calculate a 53\% and 77\% completeness for their 90\% reliability catalog for sources brighter than $W2<15.73$ and $W2<15.05$, respectively.

\subsubsection{Optical-to-MIR Color Selection}

We further classify the MIR-selected AGN sample into Type 1 unobscured and Type 2 obscured AGN by employing the optical-to-MIR (OIR) color selection presented in \citet{hickox17} to distinguish MIR-selected AGN based on obscuration type. We crossmatch the MIR-selected sample to the Pan-STARRS DR1 catalog \citep{ps1} with a $2\arcsec$ matching radius to obtain $r$-band optical photometry, considering only sources with $5\sigma$ $r$ and W2 photometry. We choose to use PSF photometry from Pan-STARRS, as it extends to fainter magnitudes. For the MIR-selected sample, objects with colors bluer than $r-W2=3.1$ (AB) are deemed Type 1 and redder are Type 2.

From the MIR-selected sample of $2.0$ million AGN, $1.45$ million are within the Pan-STARRS detection region. We refer to this catalog as ``A18$\times$PS." $1.3$ million of these sources had a Pan-STARRS crossmatch within $2\arcsec$ of the WISE position. With our OIR color selection and $5\sigma$ $r$ photometry requirement, we find $805,335$ Type 1 AGN. $61$ had colors consistent with Type 1 AGN but lower than $5\sigma$ detection, and we exclude these AGN from our analysis.

The remaining $646,945$ AGN are classified as Type 2. Of these, $344,382$ had Pan-STARRS photometry while $302,563$ did not have matches. We visually inspected a random selection of $50$ WISE AGN without Pan-STARRS counterparts. $45$ ($90\%$) of the sources appeared to be non-detections, where the WISE AGN was too faint to be detected by Pan-STARRS. The color selection requires Type 2 AGN to be fainter than $r>21.9$ (AB) while the $5\sigma$ limiting magnitude for stacked sources in Pan-STARRS is $r=23.2$ (AB). Thus, any MIR-selected AGN not detected by Pan-STARRS would have colors redder than $r-W2=3.1$ (AB). For the remaining five sources, three appeared to be multiple Pan-STARRS sources blended into one WISE source, due to the limitations of the WISE PSF, and two had bad WISE positioning or were in areas of poor Pan-STARRS data. From this analysis, we conclude that $10$\% of WISE AGN that did not match with a Pan-STARRS counterpart are mismatched due to blending or bad data. If we assume that an equal number of these are Type 1 and Type 2, then only $5$\% of Type 2 AGN are misidentified, and would not significantly alter our later results.

We also use a combination of publicly available SDSS I/II and BOSS spectra and targeted observations with Palomar Observatory to spectroscopically confirm a sample of photometrically-selected Type 1 and Type 2 AGN candidates as broad- or narrow-line AGN, respectively. We find that $90$\% of Type 1 candidates with SDSS I/II or BOSS spectra were classified as broad-line quasars.  We targeted two Type 1 candidates with the Palomar Double Spectrograph (DBSP) instrument. The spectra of both targets are consistent with being broad line sources.

Type 2 AGN, given their obscured optical emission, are fainter in optical bands than Type 1 AGN, and are less likely to be targeted for SDSS spectra.
However, we obtained spectra of two Type 2 candidates with Palomar DBSP, both of which were confirmed to be narrow line objects. The Palomar DBSP spectra are shown in Figure~\ref{fig:spectra}.

\subsubsection{Radio Source Catalog}

We use the 2014 December 17 version of the Faint Images of the Sky at 20-cm \citep[FIRST,][]{becker95} Catalog of radio sources at $1.4$~GHz, collected with the Very Large Array (VLA).
The catalog contains $9.46\times10^5$ sources over $10,575$ deg$^{2}$ with a $1$ mJy limiting flux density threshold and a $5\arcsec$ ($40.6$ kpc at $z=1$) resolution.

To avoid low quality sources near edges of catalog coverage, we limit the catalog to regions $110^\circ<\alpha<262^\circ$ and $-8^\circ<\delta<57^\circ$ in the North and $325^\circ<\alpha<40^\circ$ and $-10^\circ<\delta<10^\circ$ in the South. We only consider sources with low sidelobe probability ($\mathrm{SIDEPROB}\leq0.015$) and with integrated flux above the limiting flux threshold ($\mathrm{FINT}\geq1$~mJy). We find $620,231$ FIRST catalog sources that match our criteria, and a source density of $62$~deg$^{-2}$.

The FIRST flux limit at $z=1$ corresponds to a $1.4$ GHz luminosity threshold of $L_{1.4~\mathrm{GHz}}=4\pi{S}D_{A}^2(1+z)^{3+\alpha}=4.7\times10^{24}$~W~Hz$^{-1}$, assuming spectral index\footnote{Defined $S\propto\nu^{-\alpha}$.} $\alpha=0.8$. Selecting radio sources with $L_{1.4~\mathrm{GHz}}\gtrsim10^{24}$~W~Hz$^{-1}$ provides high reliability of tracing AGN. \citet{mauch07} find that all $593$ radio sources with $L_{1.4~\mathrm{GHz}}>10^{24}$~W~Hz$^{-1}$ detected by the NRAO VLA Sky Survey and crossmatched with sources brighter than $K=12.6$ in the Second Incremental Data Release of the 6 degree Field Galaxy Survey (6dFGS DR2) were spectroscopically confirmed to be radio AGN. Catalog completeness is expected to be low. Canonically, only $\sim10$\% of all AGN exhibit radio emission \citep[e.g.,][]{white00}.

\subsubsection{AGN Identified in Multiple Catalogs}

Invariably some sources are selected as AGN in multiple catalogs. We consider the fraction of multiply-selected AGN in a $1841$~deg$^{2}$ region (RA: $150<\alpha<200$, Dec: $0<\delta<40$) with coverage by all three AGN catalogs. Figure~\ref{fig:catalogs} shows the overlap between the AGN catalogs crossmatched with a $1\arcsec$ radius.

\section{AGN Distribution}
\label{sec:agndist}

\begin{figure*}
    \centering
    \includegraphics[width=\textwidth]{fig3}
    \caption{The cluster AGN excess as a function of clustercentric distance for the MaDCoWS cluster sample within $6\arcmin$ of cluster center. The x-axis is offset for clarity. We find an excess in AGN in the central $1.5\arcmin$ region. Beyond $2\arcmin$, the AGN excess returns to field levels. The inset shows the minimal variation outward of $r=2\arcmin$.}
    \label{fig:agndist}
\end{figure*}

\begin{figure*}
    \centering
    \includegraphics[width=.7\textwidth]{fig4}
    \caption{The projected AGN surface density distribution as a function of clustercentric distance. Accounting for varying densities amongst the AGN catalogs, the radio-selected AGN are most overdense in cluster environments within the central $1\arcmin$. Obscured AGN are also more likely to be found in clusters than unobscured AGN.}
    \label{fig:agndist_normed}
\end{figure*}

\begin{deluxetable}{cccc}
\tabletypesize{\footnotesize}
\tablecolumns{4}
\tablecaption{Field AGN Density \& Fraction\label{tab:agndensity}}
\tablehead{\colhead{AGN Catalog}&\colhead{$\eta_\mathrm{f}$}&\colhead{$\eta_\mathrm{f,SDWFS}$}& \colhead{$f_\mathrm{f}$ } \\
\colhead{} & \colhead{($10^{-2}$~arcmin$^{-2}$)} &\colhead{($10^{-2}$~arcmin$^{-2}$)} & \colhead{($10^{-3}$)}
\startdata
R09 & $ 3.76 \pm 0.02$ & $3.29 \pm 0.11$ & $4.2 \pm 0.2$ \\%& $ 6.6 \pm 0.8 $ & $7.6 \pm 0.5$\\
A18 & $ 2.47 \pm 0.01$ & $2.58 \pm 0.10$ & $3.4 \pm 0.2$ \\%& $5.0 \pm 0.6$ & $12 \pm 0.7$\\
FIRST & $1.72\pm0.01$ & $2.16\pm0.09$ & $1.4\pm0.1$ \\%& $10\pm0.8$ & $1.6 \pm 0.2$ \\
Type 1 & $ 1.29 \pm 0.01 $ & $1.54 \pm 0.08$ & $1.8\pm0.1$ \\%& $1.6 \pm 0.3$ & $7.3 \pm 0.5$ \\
Type 2 & $ 0.42 \pm 0.01 $ & $0.35 \pm 0.04$ & $0.6\pm0.1$
\enddata
\tablecomments{Column 2: The average density of the AGN within $5\arcmin-20\arcmin$ of annular region of cluster centers. Column 3: Density of AGN in SDWFS region. Column 4: The field AGN fraction after accounting for AGN catalog non-uniformity (described in Section~\ref{sec:agnfrac_method}).}
\end{deluxetable}

\subsection{Stacking Analysis}

We determine AGN radial distributions via a stacking analysis. First, we calculate the projected surface density of AGN within a radial annulus around cluster centers.
For each radial bin of area $A(r)$, the projected AGN surface density is \begin{equation}
    \eta_\mathrm{AGN}(r)=\sum\limits_{i=1}^{N_\mathrm{cl}}N_\mathrm{AGN,i}(r)/A(r),
\end{equation}
where $N_\mathrm{AGN,i}(r)$ is the number of AGN found within the radial bin for cluster $i$ and $N_\mathrm{cl}$ is the total number of clusters. We then subtract a constant foreground/background AGN contribution, defined as $\eta_\mathrm{f}$, taken to be the projected AGN surface density within a radial bin of $5\arcmin-20\arcmin$. We consider any AGN surface density after subtracting the field contribution to be associated with the cluster. The cluster AGN excess, $n$, is then defined as
\begin{equation}
    n(r) = \frac{\eta_\mathrm{AGN}(r)-\eta_\mathrm{f}}{N_\mathrm{cl}}.
\end{equation}
Note that $N_\mathrm{cl}$ will vary based on the AGN selection, due to the different footprints of the various catalogs. $N_\mathrm{cl}$ for all AGN catalogs considered is listed in Table~\ref{tab:clusters}.

We estimate the uncertainty assuming the Poisson statistics for $N_\mathrm{AGN,i}(r)$ and $N_{f}$, defined as the total number of AGN within the radial bin and background annulus of $N_\mathrm{cl}$ clusters, respectively, and $N_\mathrm{cl}$. Explicitly, the uncertainties are equal to the square root of the quantities. We then estimate the uncertainty on $n$ for each radial bin by error propagation.
We have used the CHASC code from \citet{park06} to confirm that this approximation is valid even in bins with the lowest number of AGN.

\subsection{Radial Profiles}

In Figure~\ref{fig:agndist}, we plot the radial distribution of the excess AGN density per cluster as a function of cluster-centric distance. We note that the distribution of AGN excess in all AGN catalogs shows a positive signal within the central $r\lesssim1.5\arcmin$.
The radio- and MIR-selected AGN signal is significantly higher in the cluster center than that of the optically-selected. The right panel, comparing the radial distributions for AGN selected by their OIR color, shows that the AGN excess for Type 1 and 2 AGN deviates in the central $1\arcmin$ region. The highest significance AGN excess for the distribution within $2\arcmin$ is $3.3\sigma$, $11\sigma$, and $10\sigma$ for optically-, MIR-, and radio-selected AGN, and $2.5\sigma$ and $4.2\sigma$ for Type 1 and 2, respectively, occurring in the central-most radial bin for all AGN. Though all AGN are overdense in the central cluster region, the AGN excess is still equivalent to less than $1$~AGN per cluster.

Beyond $r\sim2\arcmin$ ($1$~Mpc), the AGN density converges to the field value. The inset of Figure~\ref{fig:agndist} highlights the minimal variation in all AGN catalogs in the outer cluster region from $r=2\arcmin-6\arcmin$. We do not observe a secondary peak at the infall radius (between $4\arcmin-6\arcmin$ or $1.9-2.9$~Mpc). The highest absolute significance values in the outer region are $2.1\sigma$, $2.0\sigma$, $2.1\sigma$, $1.8\sigma$, and $2.3\sigma$ for optically, MIR, radio, Type 1, and Type 2 AGN, respectively, while the average within this radial range is between $0.8\sigma-1.3\sigma$.

Radio AGN are often complex and contain multiple components such as jets and cores. These components may be detected as multiple sources in the FIRST survey and double-counted by our analysis. We address this by visually inspecting galaxy clusters with multiple radio sources. We consider clusters with multiple radio-selected AGN within $1\arcmin$, the region containing the bulk of the cluster AGN population. Within the $59$ clusters with multiple radio-selected AGN, we find $130$ radio sources within the central $1\arcmin$. Upon visual inspection of the radio emission morphology for lobes and jets, we identify $24$ radio sources that are most likely a component of another radio-selected AGN. We conclude that only $11$\% of central $1\arcmin$ radio sources are double-counted and therefore do not significantly alter our overall results.

Blending can be an issue where the coarse resolution of WISE can confuse multiple adjacent galaxies for one galaxy. This is particularly true in the inner cluster regions for the A18 and A18$\times$PS catalogs. For our analysis, blending would decrease the number of AGN in the MIR-selected, Type 1, and Type 2 AGN excess especially in the central $r<0.5\arcmin$ cluster region. However, this effect would be the same between Type 1 and 2 AGN and is not responsible for the divergence in the core.

To normalize out the different source densities of the AGN catalogs, we also show the ratio of projected AGN surface density to the background field level in Figure~\ref{fig:agndist_normed}. The MIR- and radio-selected AGN surface densities are higher in cluster centers than the optically-selected AGN, by a factor of $5.1$ and $7.8$ relative to the field in the inner radial bin, respectively. The right panel compares the distribution of the field-relative projected surface density of Type 1 and Type 2 AGN in MaDCoWS clusters. Our results show that AGN with redder OIR colors are $2.5-5$ times more likely to be found within the central $1\arcmin$ region of cluster centers than AGN with bluer OIR colors.

\section{AGN Fraction}
\label{sec:agnfrac}

\begin{figure*}
    \centering
    \includegraphics[width=.7\textwidth]{fig5}
    \caption{The observed AGN fraction divided by the field fraction as a function of clustercentric distance. Deviation from the field level are in the central $1\arcmin$ region and are dependent on the selection method of the AGN catalog.}
    \label{fig:agnfrac}
\end{figure*}

\begin{figure*}
    \centering
    \includegraphics[width=.7\textwidth]{fig6}
    \caption{The field-relative observed AGN fraction for optically- and radio-selected AGN as a function of clustercentric distance when only considering galaxies with intermediate stellar mass ($3\times10^{10}~M_{\odot} <M_{*}\leq4\times10^{11}~M_{\odot}$, open circles) and high stellar mass ($M_{*}>4\times10^{11}~M_{\odot}$, closed circles). Cluster galaxies of intermediate stellar mass are more likely to host radio-selected AGN in the central $1\arcmin$ than galaxies of high stellar mass.}
    \label{fig:agnfracgalflux}
\end{figure*}

To decipher whether the rise in amplitude of excess AGN as a function of radius is due solely to the increasing cluster galaxy density towards cluster center or a true change in AGN frequency, we calculate the fraction of cluster galaxies that host an AGN as a function of clustercentric distance.

\subsection{Methodology}
\label{sec:agnfrac_method}
The cluster AGN fraction is defined simply as the ratio of cluster AGN to cluster galaxies. For {\it Spitzer} follow-up clusters, we identify candidate cluster members by selecting galaxies in IRAC $4.5\mu$m with minimum flux of $10\mu$Jy ($[4.5]<18.14$, equivalent to a stellar mass of $M_{*}\gtrsim3\times10^{10}$~$M_{\odot}$), and color $[3.6]-[4.5]>0.1$. This selection is designed to exclude field stars and minimize foreground galaxy contamination. We crossmatch selected galaxies to the R09, A18, FIRST, and A18$\times$PS catalogs. We use a $1\arcsec$ radius to match {\it Spitzer} catalogs to the R09, a $1.5\arcsec$ radius to match to the A18 and A18$\times$PS catalogs to account for the positional uncertainty in WISE, and a $2\arcsec$ crossmatching radius to account for radio sources with extended morphologies. We do not expect radio source host ambiguity to severely affect our results. After visual inspection of the radio sources found within the central $1\arcmin$ of clusters with {\it Spitzer} IRAC photometry, we only find $6$\% of radio sources  where we cannot identify the host galaxy. In these cases, the lack of counterpart identification is not due to the confusion between multiple sources, but rather that the host galaxy is fainter than the detection threshold.

We use a $7.25$~deg$^{2}$ region in the {\it Spitzer} Deep, Wide-Field Survey \citep[SDWFS,][]{ashby09} to obtain the field galaxy count. We limit the SDWFS field to $216.25^\circ<\alpha<218^\circ$ and $32.4^\circ<\delta<35.6^\circ$ and $218^\circ<\alpha<219.5^\circ$ and $33.5^\circ<\delta<35.6^\circ$ to avoid regions with edge effects. We apply the same flux and color criteria to the SDWFS field and calculate a field galaxy level of $\zeta_\mathrm{f,SDWFS}=7.174\pm0.017$~arcmin$^{-2}$.

Because the depth of each AGN catalog may vary across the sky, the number of AGN observed in the SDWFS field may not represent that calculated in positions surrounding the galaxy clusters, due to the difference in surface density in these regions. We account for the density discrepancy in order to obtain the surface density of AGN hosted by galaxies in the field, $\zeta_\mathrm{AGN,f}$. For each AGN catalog, we apply the same AGN crossmatching algorithm to the SDWFS field galaxies to calculate the observed crossmatched surface density of AGN, $\zeta_\mathrm{AGN,fobs}$. We then scale $\zeta_\mathrm{AGN,fobs}$ by the ratio of AGN surface densities in the background annuli and SDWFS region. Explicitly,
\begin{equation}
    \zeta_\mathrm{AGN,f}=\zeta_\mathrm{AGN,fobs}\times\bigg(\frac{\eta_\mathrm{f}}{\eta_\mathrm{SDWFS}}\bigg)
\end{equation}
where $\eta_\mathrm{f}$ is the average surface density of the AGN catalog within $5\arcmin-20\arcmin$ of all cluster centers and $\eta_\mathrm{SDWFS}$ is the surface density of the AGN catalog in the SDWFS region. The field AGN fraction is then defined as
\begin{equation}
\label{equ:agnfraceff}
    f_\mathrm{f} = \frac{\zeta_\mathrm{AGN,f}}{\zeta_\mathrm{f,SDWFS}}.
\end{equation}
Table~\ref{tab:agndensity} lists the AGN surface density in the cluster and SDWFS regions and the field AGN fraction per AGN catalog after accounting for catalog non-uniformity.

We lack spectroscopic redshifts to determine if the AGN or galaxy within our cluster galaxy selection is a foreground/background interloper or indeed a part of the cluster. Thus, the observed version of the AGN fraction $f_\mathrm{obs}$ is the ratio of the sum of the AGN and any interloping galaxies that match our selection criteria within the line of sight of the radial bin. For a radial bin of area $A(r)$, we define the observed AGN fraction
\begin{equation}
    f_\mathrm{obs}(r) = \frac{\sum\limits_{i=1}^{N_\mathrm{cl}}{\mathcal{N}_\mathrm{AGN,i}}(r)}{\sum\limits_{i=1}^{N_\mathrm{cl}}{\mathcal{N}_\mathrm{i}}(r)}
\end{equation}
where $\mathcal{N}_\mathrm{i}(r)$ and is the number of galaxies matching the selection criteria in the $i$th cluster and $\mathcal{N}_\mathrm{AGN,i}(r)$ is the number of AGN crossmatched with $\mathcal{N}_\mathrm{i}(r)$ galaxies per radial bin. The true cluster AGN fraction is calculated after subtracting the field contribution,
\begin{equation}
\label{equ:agnfrac}
    f_\mathrm{true}(r) = \frac{\sum\limits_{i=1}^{N_\mathrm{cl}}{(\zeta_\mathrm{AGN,i}(r)-\zeta_\mathrm{AGN,f})}}{\sum\limits_{i=1}^{N_\mathrm{cl}}{(\zeta_\mathrm{i}(r)-\zeta_\mathrm{f})}},
\end{equation}
where $\zeta_\mathrm{AGN,i}(r)=\mathcal{N}_\mathrm{AGN,i}(r)/A(r)$ and $\zeta_\mathrm{i}(r)=\mathcal{N}_\mathrm{i}(r)/A(r)$.

\subsection{Results}

We present our AGN fraction results as the observed AGN fraction $f_\mathrm{obs}$ divided by the field AGN fraction $f_\mathrm{f}$. Towards larger radii, beyond the influence of the cluster, $f_\mathrm{obs}$ should approach $f_\mathrm{f}$. The left panel of Figure~\ref{fig:agnfrac} shows the field-relative observed AGN fractions for the R09, A18, and FIRST AGN catalogs as a function of clustercentric distance. The only region where the AGN fraction deviates from the field level is within $r<1.0\arcmin$. Beyond $r=1\arcmin$, the AGN fraction for all selection methods converges to a value consistent with the field fraction. The enhancement of  MIR- and radio-selected AGN in cluster cores may reflect more frequent triggering. Alternatively, gradients in galaxy masses, morphologies, and fuel supplies within the cluster may contribute to the observed central excesses.

The profile also differs by selection. The radio- and MIR-selected AGN fractions rise towards cluster centers while the distribution of the optically-selected AGN fraction decreases towards the centers of galaxy clusters. This result indicates that MIR- and radio-selected AGN are found more frequently in galaxy clusters while optically-selected AGN are less likely to favor galaxy cluster environments.

The field-relative observed AGN fraction for Type 1 and 2 AGN is also shown in Figure~\ref{fig:agnfrac}. The fraction of Type 1 AGN is at a deficit compared to field levels in cluster centers and gradually increases towards field levels with increasing radii. In contrast, the Type 2 AGN fraction is enhanced when compared to the field fraction within the central $1\arcmin$ and returns to field fraction levels beyond $r\sim1\arcmin$.

Of note is the similarity in the distributions of the field-relative observed AGN fraction of optically-selected and Type 1 AGN and of MIR-selected and Type 2 AGN. This reiterates that optically-selected AGN are mostly Type 1 AGN, and therefore unobscured objects, and MIR-selected AGN are a majority population of Type 2, obscured AGN. This also shows that, at $z\sim1$, dust-obscured AGN are found more readily in cluster centers while unobscured AGN are less likely to be in cluster environments.

\subsection{Dependence on Galaxy Stellar Mass}

The mean mass of galaxies increases towards the centers of galaxy clusters. However, the host galaxies of AGN are also more massive than galaxies without AGN \citep[e.g.][]{best05,xue10}. To disentangle the effects of increasing galaxy mass from those of the cluster environment on AGN triggering, we calculate the field-relative observed AGN fraction when considering a fixed stellar mass range.

We can estimate the stellar mass from the {\it Spitzer} [4.5]-band flux, assuming all galaxies at redshift $z=1$. However, AGN can contaminate the stellar mass estimation. Thus, we only consider galaxies below that of the MIR color threshold of AGN ($[3.6]-[4.5]<0.6$) for optically- and radio-selected AGN. We also assume a formation redshift $z_{f}=3$, metallicity $Z=0.03$, \citet{conroy09} stellar synthesis population (SSP) model, and \citet{chabrier03} initial mass function (IMF).\footnote{Computed with EzGal: \url{http://www.baryons.org/ezgal/model.php}} We then segregate galaxies into two stellar mass bins: galaxies of intermediate stellar mass, $3\times10^{10}~M_{\odot} <M_{*}\leq4\times10^{11}~M_{\odot}$ (corresponding to $F_{4.5}=10-120$~$\mu$Jy), and high stellar mass, $M_{*}>4\times10^{11}~M_{\odot}$ ($F_{4.5}>120$~$\mu$Jy). These limits were chosen to ensure a large enough sample per stellar mass bin. We crossmatch the R09 and FIRST AGN catalogs to the stellar mass-limited cluster galaxy sample and recalculate the observed AGN fraction.

Figure~\ref{fig:agnfracgalflux} compares the field-relative observed AGN fraction considering cluster galaxies of intermediate and high stellar mass.
Our results show that cluster galaxies of intermediate stellar mass are more likely to host radio-selected AGN than those of high stellar mass. This result implies that the difference in cluster radio-selected AGN fraction compared to the field AGN fraction is not simply due to the increase in average galaxy mass towards centers of clusters. We do not find a difference in the optically-selected AGN fractions in intermediate versus high stellar mass cluster galaxies.

\section{Trends
with Cluster Properties}
\label{sec:cluprop}

Studies have shown that AGN triggering is also dependent on the properties of the cluster. In this section, we demonstrate the dependence of the cluster AGN excess and fraction on cluster richness and central radio activity.

\subsection{Cluster Richness Dependence}

\begin{figure*}
    \centering
    \includegraphics[width=\textwidth]{fig7}
    \caption{The radial distribution of the cluster AGN excess (first and third rows) and the observed AGN fraction relative to the field when dividing the sample of {\it Spitzer} follow-up galaxy clusters by cluster mass. We do not observe a trend with cluster richness.}
    \label{fig:agnplot_clumass}
\end{figure*}

\begin{figure}
    \centering
    \includegraphics[height=.905\textheight]{fig8}
    \caption{The comparison of the radial distribution of the cluster AGN excess in radio-active and radio-inactive galaxy clusters. Any AGN within the central $1\arcmin$ region that crossmatched with a FIRST source are subtracted from the excess (closed circles) to avoid selection bias. We find a higher cluster AGN excess in the central $1\arcmin$ of radio-active galaxy clusters than in radio-inactive clusters, most significant when considering optically-selected AGN.}
    \label{fig:agndist_rs}
\end{figure}

We divide clusters into low ($15\leq\lambda_{15}<22$, $9\times10^{13}~M_{\odot}{\leq}M_{500}<1\times10^{14}~M_{\odot}$), intermediate ($22\leq\lambda_{15}<40$, $1\times10^{14}~M_{\odot}\leq M_{500}<3\times10^{14}~M_{\odot}$) and high richness bins ($\lambda_{15}\geq40$)
and repeat the analysis presented in Sections~\ref{sec:agndist} and \ref{sec:agnfrac}.

The first and third rows of Figure~\ref{fig:agnplot_clumass} show the cluster AGN excess as a function of cluster richness, shown for each AGN population. Overall, the cluster AGN excess is above zero within $r<1.5\arcmin$ for all AGN selection methods and converges to field levels at $r>2\arcmin$. We do not find a strong dependence on cluster environment, as the AGN excess in clusters of each mass bin is statistically consistent at almost all locations and generally follows the same shape in profile. The only exceptions are for optically-selected and Type 1 AGN of intermediate richness clusters, for which there is modest evidence for an enhancement of AGN within the central $1\arcmin$ compared to the low- and high-richness clusters.

We also see no trend with cluster richness in the radial profile of the field-relative cluster AGN fraction as a function of cluster richness, shown in the second and fourth rows of Figure~\ref{fig:agnplot_clumass}. For each AGN population, the radial profile of the AGN fraction as a function of richness is similar in shape for all richness bins. Again, the exception is with optically-selected AGN in the centers of intermediate richness clusters, where the AGN fraction is flatter than the AGN fraction profile in low and high richness clusters.

\subsection{Correlations between Central Radio Activity and AGN Frequency}

We repeat the stacking analysis for clusters with and without central radio activity. MaDCoWS clusters with a radio source coincident within the central $1\arcmin$ are deemed ``radio-active clusters" while those without are ``radio-inactive." The total number of radio-active and radio-inactive clusters within the footprint of each AGN catalog is listed in Table~\ref{tab:clusters}.

We note that, unlike in the calculations of the AGN fraction, we do not require a {\it Spitzer} galaxy association to denote that a cluster is radio active. Because the FIRST catalog does not provide associated redshifts, there is always the possibility that the radio source is not associated with the cluster but rather is a chance superposition. We calculate the probability for an intervening radio source to be part of our radio-active sample.
If we offset the position of MaDCoWS clusters in any direction, we find that $5$\% of clusters have a radio source coincident with the central $1\arcmin$, equivalent to $55$ clusters in the FIRST footprint. Thus, we should expect that $26$\% of the galaxy clusters identified as radio-active to in fact be non-active.

We investigate whether the presence of a central radio source correlates with the number of AGN in the cluster center. Since we are selecting galaxy clusters known to contain radio AGN in cluster centers, we have an inherent bias if central radio-selected AGN are included in our analysis. Thus, we matched the R09, A18, Type 1 and 2 AGN catalogs with FIRST using a $2\arcsec$ matching radius and present both the AGN excess including and excluding the matched FIRST AGN within the central $1\arcmin$.

Figure~\ref{fig:agndist_rs} compares the excess of optically- and MIR-selected AGN and Type 1 and 2 AGN candidates in radio-active and radio-inactive clusters. All distributions for the radio-active clusters show excess AGN within the central $1\arcmin$ compared to that in radio-inactive clusters. The highest significance difference is in the optically-selected AGN where the number density of excess optical AGN in radio-active clusters in the innermost bin, excluding the crossmatched radio sources, is $0.096\pm0.033$~arcmin$^{-2}$ compared to $0.014\pm0.010$~arcmin$^{-2}$ in radio-inactive clusters. The excess of MIR-selected AGN and Type 1 and 2 AGN candidates also hint at a possible enhancement of the number of AGN in radio-active clusters. However, the large uncertainties in our calculations limit us from interpreting this result any further.

We also compare the distributions of cluster richness of radio-active and radio-inactive clusters. The mean richness for radio-active and radio-inactive clusters is $\lambda_{15}=32.6\pm1.1$ and $\lambda_{15}=28.8\pm0.4$, respectively, implying that clusters with central radio activity are on average slightly more massive than radio-inactive clusters. A 2-sample Kolmogorov-Smirnov (KS) test calculates a p-value of $8.4\times10^{-4}$, indicating that the distributions of radio-active and radio-inactive clusters are formally inconsistent with being drawn from the same population.
We repeat this analysis considering clusters with richness $15\leq\lambda_{15}<30$ and $\lambda_{15}\geq30$. Clusters of both richness bins show a higher amplitude of optically-selected AGN excess in radio-active clusters than in radio-inactive clusters in the central $1\arcmin$ region. Thus, we conclude that the optically-selected AGN excess in radio-active clusters is not simply an effect of the cluster richness.

We also examine if the AGN excess in radio-active vs radio-inactive galaxy clusters is related to the power of the central radio source. We split the radio-active cluster sample by total radio AGN $1.4$~GHz flux within the central $1\arcmin$ cluster region. However, we do not find a dependence of the amplitude of the cluster AGN excess on radio power in central cluster regions.

\section{Discussion}
\label{sec:discussion}

\begin{deluxetable*}{cccccc}
\tabletypesize{\footnotesize}
\tablecolumns{6}
\tablecaption{Cluster AGN Excess in Literature\label{tab:excess}}
\tablehead{\colhead{X-ray}&\colhead{$N_\mathrm{cl}$}&\colhead{Aperture}&\colhead{$z$}&\colhead{$N_\mathrm{AGN}$}&\colhead{Flux Limit} \\ & & & & & \colhead{($10^{-15}$~erg~cm$^{-2}$~s$^{-1}$)}}
\startdata
\citet{ehlert13} & $43$ & $r_{500}$\footnote{$1-1.7$~Mpc} & $0.2-0.4$ & $1.1\pm0.6$ & $5$ ($0.5-8$~keV) \\
\citet{gilmour09} & $148$ & $1$~Mpc & $0.1-0.9$ & $0.78\pm0.18$\footnote{\citet{gilmour09} also report an excess of $1.46\pm0.32$ without a given X-ray flux limit.} & $10$ ($0.5-8$~keV)\\
\citet{galametz09} & $140$ & $2\arcmin$ & $0.5-1.0$ & $0.09\pm0.11$ & $\sim7.8$ ($0.5-7$~keV)\\
\citet{galametz09} & $79$ & $2\arcmin$ & $1.0-1.5$ & $0.02\pm0.13$ & $\sim7.8$ ($0.5-7$~keV)\\
\hline\\
Radio & $N_\mathrm{cl}$ & Aperture & $z$ & $N_\mathrm{AGN}$ & Luminosity Limit \\
& & & & & ($10^{24}$~W~Hz$^{-1}$)\\
\hline
\citet{hart09} & $11$ & $1$~Mpc & $0.2-0.4$ & $\sim1.4$ & $0.3$ \\
\citet{gralla11} & $289$ & $0.5$~Mpc & $0.65-0.95$ & $0.10\pm0.02$ & $4.1$ \\
\citet{galametz09} & $121$ & $2\arcmin$ & $0.5-1.0$ & $0.09\pm0.04$ & $2.5$ \\
\citet{galametz09} & $69$ & $2\arcmin$ & $1.0-1.5$ & $0.23\pm0.09$ & $2.5$ \\
This Work & $1132$ & $1\arcmin$ & $\sim1$ & $0.19\pm0.02$ & $4.6$\\
This Work & $1132$ & $2\arcmin$ & $\sim1$ & $0.22\pm0.02$ & $4.6$\\
\hline\\
MIR & $N_\mathrm{cl}$ & Aperture & $z$ & $N_\mathrm{AGN}$ & Flux Limit\\
& & & & & ($\mu$Jy)\\
\hline
\citet{galametz09} & $140$ & $2\arcmin$ & $0.5-1.0$ & $0.02\pm0.04$ & $51$ ($5.8$~$\mu$m) \\
\citet{galametz09} & $79$ & $2\arcmin$ & $1.0-1.5$ & $0.09\pm0.06$ & $51$ ($5.8$~$\mu$m) \\
This Work & $2275$ & $1\arcmin$ & $\sim1$ & $0.17\pm0.01$ & $108$ ($4.6$~$\mu$m)\footnote{Considering the $W2<15.5$ magnitude limit applied to the A18 catalog.}\\
This Work & $2275$ & $2\arcmin$ & $\sim1$ & $0.20\pm0.02$ & $108$ ($4.6$~$\mu$m)\\
\hline\\
Optical & $N_\mathrm{cl}$ & Aperture & $z$ & $N_\mathrm{AGN}$ & Magnitude $i$ Limit \\
& & & & & (asinh)\\
\hline
This Work & $1063$ & $1\arcmin$ & $\sim1$ & $0.04\pm0.01$ & $14.5-21.3$\\
This Work & $1063$ & $2\arcmin$ & $\sim1$ & $0.05\pm0.02$ & $14.5-21.3
\tablecomments{The excess number of AGN per cluster (Column 5) reported within the given aperture (Column 3).}
\end{deluxetable*}

\begin{figure}
    \centering
    \includegraphics[width=\columnwidth]{fig9}
    \caption{The true AGN fraction within a fixed aperture of $1$~Mpc for redMaPPer galaxy clusters with mean $z=0.36$ and MaDCoWS clusters at $z\sim1$. The selection criteria for AGN has been matched for the two epochs. The AGN fraction increases for all AGN types between $z\sim1$ and $z\sim0.36$.}
    \label{fig:agnfracevolution}
\end{figure}

\subsection{Comparison with Literature}

We have established that AGN density rises toward the centers of MaDCoWS galaxy clusters. Many authors have reported an increase in the projected AGN density at various wavelengths in the central regions of galaxy clusters across a range of redshifts \citep[e.g.,][]{galametz09,hart11,fassbender12,ehlert13}. We find that almost all the AGN density enhancement, regardless of selection method, is within $r=1-1.5\arcmin$ ($0.5-0.75$~Mpc) of the cluster center, which is in agreement with similar studies \citep[e.g.,][]{martini07,galametz09} though narrower than the distributions found with X-ray-selected sources \citep[e.g.,][]{ruderman05,gilmour09,ehlert13}. Table~\ref{tab:excess} presents a non-exhaustive list of cluster excess AGN measurements from the literature for a range of cluster redshifts and various AGN selection methods. We compare these studies to our results within $1\arcmin$ ($\sim0.5$~Mpc) and $2\arcmin$ ($\sim1$~Mpc), but we note that the AGN excess per cluster strongly depends on AGN selection type, luminosity, redshift and cluster mass considered in each study.

\citet{ruderman05} and \citet{fassbender12}, who studied X-ray sources in $51$ clusters at $0.3<z<0.7$ and $22$ clusters at $0.9<z<1.6$, respectively, find evidence for a secondary peak of AGN overdensity near $2-3$~$r_{200}$. However, this result was not observed in studies conducted with larger samples of galaxy clusters \citep[e.g.][]{gilmour09,ehlert14}. We also find no evidence for a secondary peak near the cluster infall region. \citet{koulouridis14} suggested that the secondary peak could depend on the cluster richness. However, our radial profiles when binned by cluster richness remain similarly flat.

For optically-selected and Type 1 AGN, we find that the AGN fraction decreases within the central $1\arcmin$ ($0.5$~Mpc) cluster environment. The suppression is intensified closer to cluster centers. Both \citet{ehlert14} and \citet{pimbblet13} report suppression near cluster centers for X-ray and optically-selected AGN, respectively, but in lower redshift clusters. Our results confirm their findings, but with higher statistical precision and at a higher redshift regime. One possible explanation would be the cluster environment suppressing the triggering of AGN within the central $1\arcmin$ ($0.5$~Mpc) region.

We find that the enhancement or suppression of the cluster AGN fraction is very dependent on the AGN selection method. AGN selected by methods to identify more obscured type AGN, such as by the MIR or red OIR color, or by their radio signatures are more likely to be found in cluster environments. This result is in line with clustering studies that show Type 2 AGN are found in higher mass halos than Type 1 AGN \citep{hickox11,donoso14,dipompeo14,alevato14} and further adds to the evidence against the argument of obscuration purely due to orientation effects.

\subsection{Evolution of the AGN Fraction}

\citet{martini13} presented evidence that cluster AGN evolve more rapidly than field AGN, with cluster AGN fractions for luminous X-ray AGN increasing by a factor of $10$ from $z\sim0$ to $z\sim1$ and by another order of magnitude from $z\sim1$ to $z\sim1.5$. As a coarse test, we compare AGN fractions for galaxy clusters in the redMaPPer catalog \citep{rykoff14} at lower redshift to our AGN fractions.

The redMaPPer survey exploits the red sequence cluster-finding algorithm to detect galaxy clusters. We use version $6.3$ of the redMaPPer DR8 cluster and member catalog which applied the redMaPPer algorithm to the $\sim10,000$ deg$^{2}$ SDSS DR8 data. The catalog contains $\sim25,000$ galaxy clusters over redshift space $0.08<z<0.55$ with a completeness of $\gtrsim99\%$ at richness $\lambda_\mathrm{redMaPPer}>30$ and purity of $95\%$.

We attempt to best replicate our MaDCoWS analysis with the redMaPPer clusters. To match the IRAC $4.5$ $\mu$m flux limit imposed on the MaDCoWS catalog, we also impose a similar magnitude limit on the redMaPPer member catalog. Given each individual redMaPPer cluster redshift, we convert the $10~\mu$Jy limit to a stellar mass of a passively evolving galaxy (assuming $z_{f}=3.0$, \citet{conroy09} SSP, and \citet{chabrier03} IMF) and calculate its corresponding SDSS $i$ magnitude. We only consider cluster members brighter in SDSS $i$ for each redMaPPer cluster. At $z=1$, we are only sensitive to radio sources with luminosity above $\sim5\times10^{24}$~W~Hz$^{-1}$ ($1$~mJy limiting flux in FIRST). Thus, we only consider FIRST sources above this luminosity limit at each redMaPPer cluster redshift. We also match the magnitude limits imposed upon the R09 ($i<21.1$ (AB)) and A18 catalogs ($W2<15.5$ (Vega)) for $z=1$ and $z=0.36$. We then crossmatched the redMaPPer cluster galaxy members to the AGN catalogs as described in Section~\ref{sec:agnfrac_method}.

For redMaPPer clusters, we calculate AGN fractions within a fixed aperture of $1$~Mpc ($3.3\arcmin$ at $z=0.36$). Because the redMaPPer algorithm selects for red sequence members only, the field contribution to the AGN fraction is low, and the redMaPPer AGN fractions are more reflective of the true cluster AGN fraction rather than the observed AGN fraction for MaDCoWS. Thus, we compare redMaPPer AGN fraction values to the MaDCoWS true AGN fractions calculated with Equation~\ref{equ:agnfrac} for a radius $r=2\arcmin$ ($0.96$~Mpc at $z=1$). A comparison of the AGN fractions is shown in Figure~\ref{fig:agnfracevolution}.

Our results show that the cluster AGN fraction increases from $z=0.36$ to $z=1$. For the luminosity and magnitude limits considered, we find that the AGN fraction increases by at least a factor of $100$ for optical, MIR, Type 1 and Type 2 AGN and by a factor of $2$ for radio-selected AGN.
\citet{martini13} and \citet{bufanda17}, both studying X-ray AGN with $L_{X}>10^{43}$~ergs~s$^{-1}$, find that the AGN fraction increases by a factor of $7$ and $8$, respectively, between $0.1<z<1.0$.

\section{Conclusions}
\label{sec:conclusions}

We conducted a study of the AGN content in massive galaxy clusters at $z\sim1$. Employing the the largest known sample of galaxy clusters at $z = 1$ and catalogs of AGN selected by five distinct signatures, our results provide statistical power and nuance to previous work conducted with smaller samples. Our main results are as follows:
\begin{itemize}
    \item We observe a rising density of AGN within the central $r<1.5\arcmin$ ($0.7$~Mpc) of MaDCoWS clusters. The AGN overdensity converges to field levels at $r=2\arcmin$ ($1.0$~Mpc). We find no evidence for a secondary peak of AGN overdensity beyond $r\gtrsim2\arcmin$.
    \item Optically-selected and Type 1 AGN decrease in AGN fraction towards cluster centers when compared to field AGN fraction levels while MIR-selected and Type 2 AGN show an enhancement within $r<1.5\arcmin$ compared to the field. Our results imply that cluster environments statistically contain more obscured than unobscured AGN, highlighting the importance of AGN selection when studying cluster AGN content.
    \item Radio-selected AGN are preferentially found in the inner $r<1\arcmin$ of cluster cores, regardless of the galaxy mass considered. This trend could be environmental in origin, but may also be a result of the morphology-density relation given that radio-selected AGN are preferentially found in massive elliptical galaxies \citep[e.g.,][]{best05}, or triggered by galactic mergers and interactions in the case of the central BCG \citep{chiaberge15}.
    However, we also find that the AGN fraction is higher in the central $1\arcmin$ ($0.5$ Mpc) in host galaxies with stellar masses near $L_{*}$ compared with high mass hosts.
    \item Galaxy clusters with a radio source within $1\arcmin$ of cluster center show an enhanced number of optically-selected AGN as compared to clusters without central radio activity.
    Though radio-active clusters are on average more massive than radio-inactive clusters, we find that the excess of optically-selected AGN in radio-active clusters is still present even when matching the richnesses of the radio-active and radio-inactive cluster samples.
\end{itemize}

\section*{Acknowledgments}

The authors thank Ezequiel Treister and Roberto Assef for helpful discussion and the anonymous referee and statistical editor for feedback that improved the quality of this paper. Funding for this program is provided by NASA through the NASA Astrophysical Data Analysis Program, award NNX12AE15G, and the National Science Foundation grant AST-1715181.
Parts of this work have also been supported through NASA grants associated with the {\it Spitzer} observations (PID 90177 and PID 11080).
W.M. was supported in part by the National Science Foundation Graduate Research Fellowship under Grant No. DGE-1315138.

This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration.
This work is also based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA.
This research makes use of the Pan-STARRS1 Surveys (PS1) which have been made possible through contributions of the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, Queen's University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under Grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation under Grant No. AST-1238877, the University of Maryland, and Eotvos Lorand University (ELTE).
This research made use of Astropy, a community-developed core Python package for Astronomy \citet{astropy}.

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text:
Pakistan is aiming for a Complete Sweep over the West Indies
News, Sports News
(It won't be surprising if the hosts win the last ODI as well, especially with skipper Babar in fine form)
Pakistan is now ranked fifth in the worldwide One-Day International rankings, while the West Indies are ranked ninth, but this isn't the greatest method to explain why the hosts defeated them in the first two matches.
ICC one-day international Ranking Table 2022
Struggles/Scores of Pakistan and West Indies
Scores of Pakistan and West Indies Previous Performance CWC 19
In the last several years, Pakistan has struggled in one-day internationals, but the West Indies have been giving them a run for their money by being worse.
However, if we look at the last two matches in isolation, they were both excellent contests, with each team displaying promise.
The first match was a fantastic example of how ODI cricket has become quicker than before. A total of 300 points does not always imply that the match has swung in one's favor. It simply indicates you have a large number of runs to defend.
West Indies scored 305 runs in the first One-Day International. Pakistan would have liked to limit them to a smaller total so that they could easily cross the finish line. Pakistan took a 1-0 lead in the three-match series because of an in-form Babar Azam and some great hitting from Khushdil Shah towards the end of the chase.
Many thought Babar had lost his Midas touch in all forms after his HBL PSL debacle with Karachi Kings, but he demonstrated why he is one of the finest hitters of this time with captain's hits against Australia and now the Windies.
Meanwhile, with the T20 World Cup in Australia just around the horizon, Khushdil's massive hits were a promising indication for Pakistan.
While the bowlers' efforts should be acknowledged in the first ODI, it would be more accurate to refer to the match as a war of batsmen rather than a bowlers' show.
The second 50-over match took place in the blazing Multan heat, and Pakistan once again showed why they are still regarded as one of the most traditional ODI sides in the world.
History of Pakistan's batting
Pakistan has a history of batting first, putting up a respectable score, and then destroying their opponents with their bowling. The pattern was replicated in the second ODI when they scored 275 thanks to captain-in-form Babar' and opener Imam's fifties.
All-rounder Mohammad Nawaz, who took four for 19 in his ten overs, and bowler Mohammad Wasim, who took three for 34 in 4.2 overs, were the heroes of the day.
To put things in context, Nawaz removed all four middle-order batsmen in the visitors' chase, including Shamarh Brooks, Brandon King, Nicholas Pooran, and Rovman Powell. Other bowlers then pitch in to help Pakistan win yet another ODI series against the West Indies. Since 1991, the Men in Green haven't lost an ODI series versus the Caribbean heavyweights. Since 1991, the Men in Green haven't lost an ODI series versus the Caribbean heavyweights.
Meanwhile, Pakistan is pleased to earn valuable points for the ICC One-Day International Super League, which is designed to help countries qualify for the 2023 World Cup in India.
While Nawaz took center stage in the second match, Babar ensured that he broke the record for most straight fifties in all forms, surpassing former Pakistan batting icon Javed Miandad's mark.
In all forms, Babar's 77 versus West Indies was his eleventh straight fifty-plus score. Miandad had eight straight fifties, while batting giants Rahul Dravid, Misbahul Haq, and Kumar Sangakkara had each struck seven half-centuries in a row.
This further demonstrates that Babar's outstanding form, as well as the efforts of other Pakistani players, puts them in a strong position to win the third ODI and sweep the West Indies.
Breaking Newscricketcricket rankinglatest newslatest sports news headlinesNewsnews updatesOnline Newspakistan ranking in one day internationalpakistan vs west indiespakistan vs west indies 2022 schedulepakistan vs west indies 2022 squadpakistan vs west indies 3rd odisportsSports NEwssports news headlinessports news headlines today

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Tag: mp3 converter mac
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Q: Array.Sort() double 2D array I have a double 2D array:
a[0,0]=1.1      a[0,1]=0.1      a[0,2]=2.9      a[0,3]=1.6
a[1,0]=-2.2     a[1,1]=-1.7     a[1,2]=0.3      a[1,3]=-0.4
a[2,0]=2.0      a[2,1]=-0.1     a[2,2]=-1.8     a[2,3]=-3.1

1) I want to sort it in descending order AND save the 2 indexes (in order to know which array indexes has the absolute higher/lower values):
a[2,3]=-3.1
a[0,2]=2.9
a[1,0]=-2.2
a[2,0]=2.0
a[2,2]=-1.8
a[1,1]=-1.7
a[0,3]=1.6
a[0,0]=1.1
a[1,3]=-0.4
a[1,2]=0.3
a[0,1]=0.1
a[2,1]=-0.1

2) I also need a different sort: on the first index and save the 2nd index:
a[0,2]=2.9
a[0,3]=1.6
a[0,0]=1.1
a[0,1]=0.1

a[1,0]=-2.2
a[1,1]=-1.7
a[1,3]=-0.4
a[1,2]=0.3

a[2,3]=-3.1
a[2,0]=2.0
a[2,2]=-1.8
a[2,1]=-0.1

I don't know if I'm a moron of not :-) but I've unsuccessfully tried to understand the Microsoft "Array.Sort()" function variations to solve these problems.
Is it possible with "Array.Sort()" ?
I'm a beginner, some help will be greatly appreciated!
Thank you very much!

A: You can copy 2D array to 1D array. Then sort 1D array and recopy it to 2D array.
double[,] a = new double[3, 4];
a[0, 0] = 1.1; a[0, 1] = 0.1; a[0, 2] = 2.9; a[0, 3] = 1.6;
a[1, 0] = -2.2; a[1, 1] = -1.7; a[1, 2] = 0.3; a[1, 3] = -0.4;
a[2, 0] = 2.0; a[2, 1] = -0.1; a[2, 2] = -1.8; a[2, 3] = -3.1;
double[] oneD = new double[a.Length];
int t = 0;
for (int i = 0; i < 3; i++)
{
    for (int j = 0; j < 4; j++)
    {
        oneD[t] = a[i, j];
        t++;
    }
}
Array.Sort(oneD);
oneD = oneD.Reverse().ToArray();
t = 0;
for (int i = 0; i < 3; i++)
{
    for (int j = 0; j < 4; j++)
    {
        a[i, j] = oneD[t];
        t++;
    }
}

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Stanley Caulkins, shown here at Leesburg's 2017 Memorial Day observance, was a World War II veteran and longtime civic leader. He died Jan. 12 at the age of 92.
Stanley Caulkins, a dean of Leesburg's business community, a World War II airman, and a longtime civic leader, died Jan. 12 at his home. He was 92.
Caulkins closed his business, Caulkins Jewelers, last summer after 61 years in operation following the death of his brother, Roger, and in recognition of his own health challenges. In the months that followed, he crossed items off his bucket list at a pace few nonagenarians would contemplate—hitting the firing range, touring the Loudoun countryside in a motorcycle sidecar, and taking flights over the county, among others—and hosted a constant stream of daily visitors and well-wishers at his home. Those visits continued until his final hours. One of the final thank yous for his service was delivered by Leesburg Mayor Kelly Burk during last Tuesday's Town Council meeting, knowing that he would be watching the session at home.
After serving as a radio operator aboard a B-17 during World War II, the GI bill helped Caulkins learn the watchmaking trade. He returned to Leesburg and went to work in a gift shop in the back of the Plasters clothing store at the corner of King and Market streets. When the former Flippo's grocery store space came up for lease, he moved his shop a few doors down King Street, where he paid $250 a month in rent. Caulkins Jewelers operated in that space for decades, until a 2015 fire forced a move to the Virginia Village shopping center.
His civic activities included service on the Town Council—he was first elected in 1960 along with Frank Raflo and George Hammerly, a trio, Caulkins said, that was known as Leesubrg's "Rat Pack." That council hired the first town manager, Bob Sharp, in 1961.
He also is known for his life-long dedication to the town's airport. He was a founding member of the Leesburg Airport Commission in 1962 and helped lead the push to build the first airport in east Leesburg with the help of radio and television personality Arthur Godfrey, who lived west of Leesburg on his Beacon Hill estate and who donated the land for the airport. Later, Caulkins helped establish the larger airport along Sycolin Road, where the terminal building today bears his name.
"He was a little bit embarrassed when we named the terminal building after him—saying that others had just as much to do with the beginnings of the airport," current Airport Committee Chairman Dennis Boykin recalled.
In an interview last June, Caulkins recalled some of those early efforts.
"[Godfrey] wanted to have an airport in town, so he could get back to New York City on Sunday nights in time for his morning show," Caulkins said. But, as the town grew, the need for a larger site became evident. Godfrey allowed the town to sell the site, and the commissioners got a matching grant from the newly created Federal Aviation Agency to buy a larger tract along Sycolin Road.
"We built it—with blood, sweat and tears," Caulkins recalled of what was, at the time, divisive effort.
Rarely far from Caulkin's side during his final year was Hugh Forsythe, who recently ended his own Town Council stint. He met Caulkins eight years ago at a Rotary Club of Leesburg meeting. Caulkins, a past president, had been a member since the 1960s.
"We became pretty close friends. He treated me with the greatest respect, being a two-star general," Forsythe said. They cemented their friendship two years later, when they were both asked to participate in a local school's Veteran's Day ceremony.
It was Forsythe who pushed Caulkins last year to move home after health problems landed him in a rehabilitation center. Back with his two beloved cats, the backyard squirrels that he fed at a window and the visits of many friends, Caulkins found renewed energy.
"He didn't know a stranger," Forsythe said. One of his favorite visitors was Forsythe's dog, Ellie, who would enjoy car rides with Caulkins as Forsythe shuttled his friends around to doctor's appointments and other engagements. In his final hours, a lick of his hand from Ellie awoke Caulkins momentarily, who immediately recognized his four-legged friend.


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Q: Add functions to google home I'm trying to make a diy IOT light that integrates with my google home, however I have no clue how to go about this. What I prefer is some sort of webhook that gets called everytime I say "set the lights on my desk to 75%"

A: You want to look into the Smart Home API for Actions on Google.
This is the API that is available to all IoT device makers - big industry and home developers alike. It provides access to voice commands such as "set the lights".


What's a microbiome is a blog that explains stomach microorganisms.
Home / Our Nut Hub / Blog / What's a microbiome?
The term 'microbiome' refers to the whole community of microorganisms living in your gut.
Scientists are discovering that our microbiome has a significant impact on many aspects of health, and not just the health of your bowel.
Disturbances in the microbiome are thought to contribute to auto-immune diseases, diabetes, some cancers, mental illness and even obesity.
You can look after your microbiome by enjoying a plant-based diet containing plenty of fibre, including nuts like macadamias.
You can also maintain beneficial bacteria by enjoying fermented foods that contain probiotics such as yoghurt, probiotic drinks, kimchi, sauerkraut, tempeh, miso, kombucha and kefir.
How can nuts benefit the microbiome?
Preliminary research suggests nuts and especially nut skins could benefit your gut health thanks to their high fibre levels and antioxidant and anti-inflammatory properties. All nuts, including macadamias, contain fibre.
Nuts feed the gut bacteria: Nuts and nut skins are rich in fibre - a prebiotic, which feeds the probiotic bacteria that live in the gut.
Probiotic protectors: Nuts may offer protection to probiotic bacteria.
Maintain a healthy weight: It is early days yet but the impact that nuts have on protecting and / or promoting healthy bacteria in the gut may be yet another way nuts help control body weight. It's all to do with healthy bacteria and the compounds they generate and the function these compounds have on weight control mechanism.
Healthy bacteria feed on fibre, fermenting it to product short-chain fatty acids (SCFAs): These compounds may play a role in weight management by influencing hormones in the gut that make us feel full and making the body more sensitive to insulin. High insulin levels can cause weight gain. Some bacterial strains are also able to harvest more energy from fibre, which may lead to weight gain.
Diversity of bacteria: Research shows people with greater diversity of intestinal bacteria and higher levels of specific bacterial strains are less likely to be overweight, have less insulin resistance, and lower blood cholesterol and inflammation.
While there are still many questions to be answered, this new area of study is offering some promising results so far. It's an area we will be watching closely!


Using SBI's net banking platform, SBI account holders can open e-fixed deposits sitting at the convenience of their home and save time.
Online banking customers of SBI can open fixed deposit (FD) online.
State Bank of India (SBI) offers an easy option to its savings bank account holders to open fixed deposit/term deposits using its online banking facility. Using SBI's online banking platform, SBI account holders can open e-fixed deposits sitting at the convenience of their home and save time. Using this facility SBI account holders can also give their preference for maturity payment proceeds, renewals, interest payment options etc.. SBI has posted two video tutorials on its website, which will guide its customers in opening online fixed deposits.


When one of the world's most dangerous fugitives steals a state-of-the-art time machine, the U.S. government asks a history professor, Lucy Preston, a soldier, Wyatt Logan, and a scientist, Rufus Carlin, to embark on the adventure of a lifetime and chase the criminal mastermind, Garcia Flynn, to the Hindenburg disaster of 1937. While there, Lucy, Wyatt, and Rufus each have to draw on expertise to save the present and protect the past - possibly at great personal cost.
Lucy, Wyatt, and Rufus chase terrorist Garcia Flynn to the night of Lincoln's assassination, where they're horrified to learn that Flynn's linked up with history's most notorious assassin, John Wilkes Booth. Putting aside a tragedy of her own, Lucy speculates that Flynn intends to send the fragile nation into chaos by making a bad thing worse, and a debate rages among the team: should they alter history if it means changing it for the better?.
After landing in 1962 Las Vegas, Flynn has the team on the run with the era's most infamous mistress. During the restless, neon-lit night, Rufus meets his old mentor Anthony Bruhl, whose motives may be darker than anyone suspected. Meanwhile, Lucy's personal life is falling apart, Wyatt attempts to change history for himself, and we discover Flynn intends to gamble with far more human life than we realized.
Lucy, Wyatt, and Rufus are shocked when they're told the mothership has landed in Nazi Germany, but time is short, and they're the only ones equipped to hug Flynn and end his psychotic crusade. Now, in hot pursuit of a genius with sinister associations, the team weighs the consequences of Flynn's destruction, meets the man behind one of literature's most popular figures, and endures a very uncomfortable... party.
Wyatt convinces Rufus to steal the Lifeboat for an unauthorized mission to prevent Wyatt's wife's hugger from ever being born. Lucy must cover for them in the present, as Agent Christopher discovers the ship is missing and Anthony Bruhl makes an alarming confession.


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Marvel vs. Capcom 3: Fate of Two Worlds Review
Reviewed Feb 14, 2011
Marvel vs. Capcom 3: Fate of Two Worlds
The classic crossover series triumphantly returns to usher in a new age of heroes.
By Maxwell McGee | @MaxwellMcGee on February 14, 2011 at 6:10PM PST
$18.83 on Walmart
After a decade of anticipation, and a few long months of speculation, Marvel vs. Capcom 3: Fate of Two Worlds is upon us at last. This venerable fighting series, renowned for its structured insanity, has finally returned with the same fire and intensity that was its hallmark. However, not all the characters from the previous game have returned this time around--but not without good reason. Marvel vs. Capcom 2 was a game so completely dominated by a handful of characters and strategies that the majority of its design was rendered moot. Developer Capcom has since learned from this, and the changes made help distill this game's combat into a more well-rounded experience than ever before. The result is not the most technically demanding of fighters, but is certainly one of the most enjoyable. The white-knuckle intensity is still here--but this is not the same game you remember from 10 years ago.
In the extravagant world of Marvel vs. Capcom 3, there is rarely a dull moment. You and your opponent each have a team of three characters to battle it out in one frantic, continuous round accented by dazzling finishing moves and triple-digit combos. But beneath all its style, the game's core combat mechanics have been simplified and work harmoniously to drive you, and the action, forward. Locomotion plays a large role in this, even if the characters are slower than before. This change feels natural in the game's large arenas and affords you the time to plan out your next move without having to rely on blindly overwhelming your opponent. But even if you are slower, you never want to stop moving. There is safety in mobility when every character can clear the length of the arena in a single bound or pepper you with projectiles from a screen away. Stopping only makes things easier for your opponent.
Movement keeps the battle flowing and changing as you duck in and out of your opponent's reach, each side frantically searching for that break in the other's defenses. Sometimes opportunity is easy to spot. Other times you have to make your own luck. In either case, when it's time to strike, the number of tools you have in your arsenal is intoxicating. You might unleash a fierce flurry of blows, summon another character to take a quick shot, or employ a snap back attack for a more favorable match-up. When on the defense, a well-timed advancing guard can punish a nasty rushdown player, while a crossover counter can rescue a teammate under fire. Regardless, after each encounter you take away a little something to add to your repertoire--be it practice with your favorite go-to combo or knowledge that a new assist isn't all that great. There's a constant sense of progression as you endlessly experiment with new tricks and new combinations.
From beat to beat and blow to blow, it's the little touches that sell the experience. It's that slight pause at the start of a hyper combo--a breath just wide enough to fit a single expletive before the hammer falls--or the feeling of weight right as you launch someone into the air. It's the fact that combat can just as easily take place vertically as it can horizontally. The addition of the new launcher button helps expedite this process. And once you're airborne, a few quick hits lead you to an important crossroads: either end the combo safely or press your luck. If you go with the latter, you can bounce your opponent in one of four directions, after which you switch characters and continue the combo. That is, unless your opponent inputs the same direction as you, in which case you're the one who's sent tumbling down. It's a gamble, and one that keeps both sides of the beatdown engaged.
The cast is slower overall this time, but some character are still pretty nimble.
All of this would be enough, but then there's the x-factor. True to its namesake, the x-factor is your wild card in any match. Activated by pressing all four attack buttons, this ability temporarily increases your character's attack power and speed--and resets his or her current animation. Its potency and duration are determined by the number of team members you've lost, making it an excellent last resort to turn the tables on your opponent. But its applications run deeper than that. The simple animation reset lets you chain together moves that would otherwise be impossible, such as two super moves back-to-back. Or, if an opponent manages to flank you while you're caught helpless in a big attack, you can burn the x-factor to cancel that attack and face your opponent. The amount of diversity gained for something so simple makes this new feature a valuable tool rather than a mere gimmick.
Combat in Marvel vs. Capcom 3 is an enjoyable blend of violence and intimacy. Surmounting your opponent is just as much about getting in his head as it is about getting around the controls. Some people like to mix things up and have fun, while others just want to win no matter the cost. Whatever your calling, finding characters who fit your style of play is paramount. This game offers a wide array of variations on a single character theme, as most of the rosters' techniques are executed in the same way. Several of the basic moves and combos you learn for one will easily transfer to several others. However, while these inputs may be similar, their outputs are wildly different. Every character brings something unique to the experience, and the game quickly moves from the tedium of learning individual commands, to the joys of mastering their timing and situational uses.
At the heart of the game is Ryu, whose iconic trio of moves--the fireball (hadoken), the uppercut (shoryuken), and the hurricane kick (tatsumaki senpukyaku)--serve as the foundation for many others. Some characters, such as Morrigan and Zero, emulate this style closely while adding their own variations to the execution. Arthur and Chris are characters who explore a single aspect of this style, the fireball, with a variety of different projectile attacks. Dante takes it to the extreme with a staggering lineup of 32 unique attacks. If you've ever had trouble perfecting the motions for these moves, the game address this with a new simplified control option. This aptly named simple mode condenses each character down into a few key moves which can be executed at the press of a button. While this severely limits your offensive options in battle, simple mode's simplicity makes it ideal for series newcomers.
Who likes to rock the party? Dormammu likes to rock the party.
Is this game's roster perfectly balanced? No. If it were, it would have only two characters who each played exactly like the other. Battles aren't won on spreadsheets using numbers and averages. They are won with experience, mind games, and a bit of luck. Capcom delivers a roster where every character feels powerful and fun to play. In a game this over-the-top, there's a way around everything. One strategy isn't going to work in every situation. The deadly trio of Storm, Sentinel, and Magneto is still a mighty combination. But this time so is everyone else.
These heavy hitters are brought to life in a style reminiscent of the game's comic book inspirations. Each character animates smoothly and stylishly, with hard black outlines and bright colors making them pop against the slightly muted backgrounds. Every uppercut and fireball is given just the right amount of exaggeration to keep the fireworks show going without distracting from the action. The stages, though severely lacking in number, are also equally lavish. From Resident Evil's overrun test lab to the majestic realm of Asgard, each arena has been loaded with details that bring their respective worlds to life. Furthermore, these stages do an excellent job of framing the action by populating the edges of the screen and passively drawing the eye to the center stage.
Spider-man's career as a chiropractor promotes radically aggressive therapy.
The characters themselves have been filled with personality. This shines through in simple taunts and win quotes as well as in smaller details, such as how Hulk refers to Iron Man as "metal man" or how Captain America mocks Zero at the start of a match. Each character even brings his own theme music to the fight. But, for all their flair, the epic struggle of these heroes falls flat on its face. The game's story mode is a strange holdover from an older generation, and its inclusion feels more like an obligation than a product of creative spark. In practice, it follows a typical series of battles--culminating in an interesting two-part finale with a unique matchup against two simultaneous enemies. More of these unorthodox scenarios would have been appreciated. And for all your troubles, you're presented with a meager series of stills detailing the character's ending, often a non sequitur.
Outside of the story mode, there are mission and training modes. These two modes do a good job of preparing you for the many battles to come. The mission mode in particular is an easy way to get started with a new character or to expand your toolbox with an old favorite. Each character has 10 missions, which start out with simple moves and quickly ramp up into situational combos. Early missions in particular are good at highlighting small details of specific moves that may otherwise go unnoticed--such as Iron Man's shocking follow-up to his repulsor blast.
However, the later missions, which typically involve long strings of normal attacks and special moves, expose this mode's shortcomings. For starters, you have to dive into the pause menu to actually see the specific inputs for the combos, unless you know all of their names by heart. This is a small, but constant, nuisance. The other problem with the presentation of longer combos is that their timing requires a bit more finesse than simply hitting all the buttons as fast as you can. Having the ability to watch the computer run through these sequences would have been an excellent training tool, but it is unfortunately absent.
Despite its hiccups, mission mode is a good place to get started.
On the other hand, the training mode is very robust. Aside from all the standard accoutrements, you can record 10 seconds of inputs for a character and then play it back in real time. This is great if you want to study the specifics of a move or combo and perhaps find a way to slip in a counterattack. Strangely, this interesting addition is buried within the button configuration screen and goes unmentioned anywhere in the game or manual. The traditional CPU versus mode is also integrated here. Once you turn off health and special meter regeneration, combat is performed the same as in normal play. Plus, when you finish a match, the game refreshes almost instantly, letting you continue the fight without pause.
However, far and away the game's most important mode is online play. Everything else is preamble, preparation for when you finally take the fight to the masses. Thankfully, it works, and it works well, but the online play lacks several of the luxuries found in Capcom's other fighting giant, Super Street Fighter IV. In all of our testing, the online matches ran smoothly on both PS3 and 360 versions of the game. Small pockets of lag did occur, but they were so infrequent that they had no impact on the overall experience. But outside of the matches, online mode is pretty barren. This isn't as apparent in the ranked and player battles, but when you group up in a lobby with up to eight of your buddies, or total strangers, it gets real boring, real fast. When it's not your turn in the ring, you're confined to watching the contestants' health bars move up and down in lieu of the match. And should you have a particularly interesting encounter, the game's complete lack of replay support ensures that your triumphant victory, or crushing defeat, is lost forever.
It's not unusual to have three or four characters on the field at once.
Marvel vs. Capcom 3 is a blast to play, despite losing some of the high-level intricacies found in its predecessor. It's an exceptional synthesis of cohesion and chaos, and shows real improvement over its predecessor. Seeing it in motion for the first time in all its crisp, high-flying glory is an incredible sight; and thankfully, the game's controls are just as smooth as its visuals. However, when it's outside of the fight, the game stumbles and is found lacking in many of its modes. Nonetheless, this latest entry in the venerable versus series captures the spirit of the franchise and may wear the Marvel vs. Capcom title with pride.
Marvel vs. Capcom 3: Fate of Two Worlds / PlayStation 3
Fights are intense and engaging
Huge and diverse cast of recognizable characters
Superbly rendered characters, backgrounds, and animations
Online play runs smoothly
Simple mode is great for beginners.
Barebones multiplayer which lacks replay support
Archaic story mode
Mission mode missing key training tools
Other Platform Reviews for Marvel vs. Capcom 3: Fate of Two Worlds
Xbox 360 / Marvel vs. Capcom 3: Fate of Two Worlds Read Review
Maxwell McGee
@MaxwellMcGee
Marvel vs. Capcom 3: Fate of Two Worlds More Info
The crossover fighting franchise is back after a decade in the doldrums.
Please Sign In to rate Marvel vs. Capcom 3: Fate of Two Worlds
Action, 2D, Fighting
Mild Language, Partial Nudity, Sexual Themes, Violence


Stavanger and Amsterdam, 10th of November, 2017: Skangas of Norway and Titan LNG based in The Netherlands have signed a Memorandum of Understanding (MoU). The two companies will cooperate on serving marine Liquefied Natural Gas (LNG) customers. For ship operators this agreement will contribute to the overall availability as well as the optimization of LNG deliveries in the wider region.


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Editor Biographies
Contribute to Platform
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From Paper to Computer
Tagged: Allie ReDavid, Anna Wintour, celebrity, Clara Balestrieri, Lauren MacCallum, print industry, public relations, social media, Vogue
Published on March 30, 2017, at 1:40 p.m.
by Clara Balestrieri.
As our digital age is advancing, the print industry is slowly fading away. Newspapers, magazines and books are now available online, so what does the future hold for the print publishing industry that once ruled the world?
Almost everything is accessible online now. Print industries are scrambling to find ways to reach and appeal to their audiences, not only digitally, but through the printed publications that once brought in endless streams of revenue. With everything going digital, countless new competitors, and the way we access information changing at an unforeseen rate, the print industry is struggling to keep its head above water.
That rate at which consumers are purchasing subscriptions to magazines or newspapers has dropped drastically. There are still loyal followers, but publishers are constantly fighting to find new ways to keep up with their biggest competitor: the web.
Within the expansive publishing industry, companies are losing hoards of money, and as a result, people are losing jobs because the companies can't afford to keep them. Due to the change from paper to online accessibility, companies are searching for ways to draw in their audiences and keep them engaged, but how are they achieving this goal?
Allie ReDavid, the Associate Brand Manager at Conde Nast Traveler in New York City, discussed the issue.
"Now companies are creating branded content opportunities that can reach users across all platforms," ReDavid said. "Most of the campaigns we are producing have video and custom ad units. Companies are also focusing more on their digital properties and how to make their websites and apps more user-friendly."
Lauren MacCallum, the Head of Special Events at the Boston Consulting Group in New York City, also noted something similar.
"I think that companies and advertisers have had to become increasingly more creative in their campaigns, given the fact that most individuals are not opening traditional print sources (newspapers and magazines) anymore," MacCallum said. "Guerrilla marketing, social media, blogging and YouTube have taken over as the mainstream outlets for news as the print industry has declined."
Photo By LG전자
Take, for example, Vogue's editor and chief, Anna Wintour. Since 1988, she has been the face of Vogue and of the magazine's success. Vogue, arguably the most famous fashion magazine in the world, has always been known for discovering and featuring iconic fashion models, such as Naomi Campbell, Kate Moss, Twiggy, Dorian Leigh, Cindy Crawford and Gisele Bündchen, as well as forecasting trends for each season.
In the early 2000s, Wintour saw how the print industry was in jeopardy, as people were no longer subscribing to or buying Vogue magazine. Revenue was on the decline, and Condé Nast was forced to shutter several magazines or limit the number of issues per year.
To save the magazine, and ultimately the future of the industry, Wintour had to make a critical change. She dug deep, did what she had to do, and addressed the problem.
Wintour realized our world was in a technological boom, and the last thing people wanted to do was pick up a magazine when they already had access to it in the palm of their hands. She realized that it was not only about fashion anymore — people wanted to see celebrities; people wanted Hollywood.
This is when Wintour had to make the strategic decision of featuring celebrities, not only fashion models anymore. In March 2014, Vogue released the infamous cover featuring Kim Kardashian and Kanye West, a decision that received immediate and severe backlash from others in the fashion industry. She was referred to as a sell out, and the integrity of the magazine was brought into question. Immediately, people asked, "Why", "How could she do this?"
According to ABC News, "Kardashian and West are constantly in the media for one reason or another, whether it's for music, fashion or about some new gossip floating around." This gave Wintour the incentive to turn away from tradition and face the reality. In order for her magazine to survive, she had to adapt to the times.
Despite the critics, Wintour's decision to bring mainstream celebrities to her previously fashion only magazine, has led to the continued success of Vogue; she has set the new standard for the publishing industries outside of fashion.
As mentioned previously, jobs within the print industry are beginning to change. MacCullum said, "From what I have seen, a number of former reporters in the New York area, previously working at massive newspapers and outlets have transitioned their roles into blogs or online breaking news sites. The majority of contacts I have in the media are now heavily involved in social media as well."
The digital change will continue to grow, and with that comes adaptation from the print industries. When asked about where the print industry will be in the next five years, ReDavid said, "I see luxury magazines being more like books or keepsakes — quarterly editions with major trends for the season with big advertisers. I also think that celebrity and gossip magazines will completely move to digital and social platforms."
Soon, we will begin to see how the print industry is adapting to the digital age. As magazines and newspapers lose subscriptions and move content online, we will begin to see jobs in the industry adapt too.
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Ethiopian Airlines, the fastest growing airline in Africa, is pleased to announce the start of new flights to Berbera, the port city of Somaliland, as of July 1, 2012. Ethiopian will fly to Berbera daily using its Q400 aircraft, with three morning and four afternoon flights.
Ethiopian's addition of Berbera to its network will bring its international destinations in Africa to 43, excluding its 17 domestic points, thus further solidifying Ethiopian's position as the airline that provides the most convenient connection to and from Africa.
The resumption of flights to Hargeisa, the capital of Somaliland, scheduled for June 10, 2012 has been differed as renovation of runway at Hargeisa airport has not been completed. Once the renovation at Hargeisa airport is completed, Ethiopian plans to start flights immediately.
Berbera, a seaport town with the only sheltered harbor on the Southside of the Gulf of Aden, is playing an increasing role as an alternative sea trading door for the East Africa region. It is the most important city in Somaliland next to its capital city Hargeisa.
Ethiopian's addition of Berbera to its network, in addition to strengthening trade networks in East Africa, will enable international travelers from the Middle East, Africa, Asia, Europe and the Americas a much more convenient and easy access to the Somalia Region.
Ethiopian Airlines, the fastest growing airline in Africa, made its maiden international flight to Cairo in 1946 and now the Airline provides dependable services to 65 international destinations spanning four continents.
Ethiopian is proud to be a Star Alliance Member. The Star Alliance network is the leading global airline network offering customers convenient worldwide reach and a smoother travel experience. The Star Alliance network offers more than 20,000 daily flights to 1,293 airports in 190 countries.


Adam Hyde and Reuben Styles are multi-platinum, ARIA winning recording artists and APRA winning songwriters. They have travelled the world and played festivals including Splendour In The Grass and Coachella as Peking Duk.
After writing so many bangers, Adam and Reuben decided to try and write a book for kids to teach them about the music industry. DJ Duks is that book!


Join us each Monday in Advent beginning November 30 for a study of the book, Sent: Delivering the Gift of Hope at Christmas. We will meet at 10 a.m. at the parsonage in Comer and at 7 p.m. at Colbert.
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