text:
\section*{List of Contributors}

\section*{Abstract}
The intra-cluster and inter-galactic media that pervade the large scale structure of the Universe
are known to be magnetised at sub-micro Gauss to micro Gauss levels and to contain cosmic rays.
The acceleration of cosmic rays and their evolution along with that of magnetic fields in these media is
still not well understood.
Diffuse radio sources of synchrotron origin associated with the intra-cluster medium
(ICM) such as radio halos, relics and mini-halos
are direct probes of the underlying mechanisms of cosmic ray acceleration.
{Observations with radio telescopes such as the Giant Metrewave Radio Telescope,
the Very Large Array and the Westerbork Synthesis Radio Telescope have led to the discoveries of about
80 such sources and allowed detailed studies in the frequency range 0.15 - 1.4 GHz of a few.}
These studies have revealed scaling relations between the thermal {and non-thermal} properties of clusters and
favour the role of shocks in the formation of radio relics and of turbulent re-acceleration in the formation of
 radio halos and mini-halos.
The radio halos are known to occur in merging clusters and mini-halos are detected in about half of the
cool-core clusters.
Due to the limitations of current radio telescopes, low mass galaxy clusters and galaxy groups
remain unexplored as they are expected to contain
much weaker radio sources. Distinguishing between the primary and the secondary models of
cosmic ray acceleration mechanisms  requires spectral measurements
over a wide range of radio frequencies and {with high} sensitivity. Simulations have also
predicted weak diffuse radio sources associated with filaments connecting galaxy
clusters.

The Square Kilometer Array (SKA) is a next generation radio telescope that will operate in
the frequency range of 0.05 - 20 GHz with unprecedented sensitivities and resolutions.
The expected detection limits of SKA will reveal a few hundred to thousand new radio halos, relics and
mini-halos providing the first large and comprehensive samples for their study. The wide frequency coverage
along with sensitivity  to extended structures will be able to constrain the cosmic ray acceleration mechanisms.
The higher frequency  ($>5$ GHz) observations will be able to use the Sunyaev-Zel'dovich effect to probe the ICM
pressure in addition to the tracers such as lobes of head-tail radio sources.
The SKA also opens prospects to
detect the ``off-state'' or the lowest level of
radio emission from the ICM predicted by the hadronic models and the turbulent re-acceleration models.

\section{Overview}
The Square Kilometer Array (SKA) is the next generation radio telescope
that will probe the fundamental physics of formation and evolution of galaxies up to
large scale structures in the Universe.
The SKA has a low frequency component (SKA1-low\,\,) that will be built in Australia and
a high frequency component (SKA1-mid\,\,) to be built in South Africa.
This document gives an overview of the scientific interests of the Continuum Science Working Group
members of SKA India in the field of galaxy clusters and the cosmic web.

\section{Current SKA1 parameters}
A brief description of the currently planned SKA1-mid and the SKA1-low telescopes is
provided below. The complete details can be
found in the SKA document
released in November 2015
\footnote{SKA-TEL-SKO-0000308\_SKA1\_System\_Baseline\_v2\_DescriptionRev01-part-1-signed.pdf.
Note that the ``SKA1-SUR'' for which predictions can be found in
the articles in AASKA 2014 book has been deferred.}.

\subsection{SKA1-mid (0.35 - 13.6 (20) GHz)}
The SKA1-Mid telescope is proposed to be a mixed array of 133 15-m SKA1 dishes and 64 13.5-m
diameter dishes from the Meer Karoo Array Telescope (MeerKAT). The antennas will be arranged in a moderately compact core with a
diameter of $\sim$1 km, a further 2-dimensional array of randomly placed dishes out to
$\sim$3 km radius, thinning at the edges. Three spiral arms will extend to a radius of
$\sim$80 km from the centre.\\
The dishes will be capable of operations up to at least 20 GHz, although initially equipped to
observe only up to 13.8 GHz for SKA1. MeerKAT dishes are expected to be equipped with a front-end
equivalent to SKA Band 2 (0.95 - 1.76 GHz), a Ultra High Frequency front-end that overlaps with Band 1 (0.3 - 1 GHz),
and an X-band front-end (8 - 14.5 GHz).
Band 2 (0.95 - 1.76 GHz), 5 (4.6 - 13.8 GHz) and 1 (0.35 - 1.05 GHz) will be constructed in priority order as written
and the sensitivity at a fiducial frequency of 1.67 GHz is given in Table ~\ref{skasens}.

\subsection{SKA1-low (0.05 - 0.35 GHz)}
SKA1-low telescope receptors will consist of an array of $\sim$131,000 log-periodic
dual-polarised antenna elements. Many of the antennas will be arranged in a very compact
configuration (the `core') with a diameter of $\sim$1 km, the rest of the elements will
be arranged in stations, each a few 10s of metres in diameter. The stations will be distributed
over a 40-km radius region lying within Boolardy Station, most likely organised into
spiral arms with a high degree of randomisation.\\
The antenna array will operate from 50 MHz to $\sim$350 MHz.\\
The antenna elements will be grouped into $\sim$512 stations, whose antennas will
be beam-formed to expose a field-of-view of $\sim$20 deg$^{2}$. The expected sensitivity at
a fiducial frequency of 0.11 GHz is given in Table ~\ref{skasens}.

\begin{table}[t]
\centering
\caption{Sensitivities of SKA1 as of Nov. 2015.}\label{skasens}
\begin{tabular}{lcccccc}
\noalign{\smallskip} \hline
\hline \noalign{\smallskip}
 &$\nu^{\dag}$& BW&rms&$\theta_b$ \\
 &GHz &MHz&$\mu$Jy b$^{-1}$ hr$^{-1/2}$& arcsec\\
 \hline \noalign{\smallskip}
SKA1-mid\,\, &1.67&770&0.75&0.25\\
    \hline \noalign{\smallskip}
SKA1-low\,\, &0.11&300&3.36&7\\
 \hline
 \hline
\end{tabular}\\
$^\dag$ Fiducial frequencies as provided by the SKA are used here.
\end{table}

\section {Introduction: Galaxy clusters, groups and superclusters}
\label{gal-cluster}
The theorized large scale structure of the Universe evolving through initial density fluctuations
\citep[e.g.][]{1970A&A.....5...84Z} has been observed to be a
network of filaments and sheets of matter \citep{2003ApJS..148..175S},
interwoven like a `web' \citep{1996Natur.380..603B} and has been reproduced by cosmological
simulations \citep[e.g.][]{2005Natur.435..629S}.
Galaxy clusters are the nodes of the `web' having typical masses $\sim10^{14-15}$ M$_{\odot}$ and
 containing hundreds to thousands of galaxies moving with velocities $\sim700 - 1000$ km s$^{-1}$
 \citep[e.g.][]{1993ApJ...404...38G}.
Diffuse thermal gas of temperature $\sim10^{7-8}$ K (a few keV) at cluster cores
emits thermal Bremsstrahlung making clusters extended, soft X-ray emitting sources
\citep[e.g.][]{1966ApJ...146..955F,
1977MNRAS.178P..75M}. This thermal plasma also contains relativistic particles (GeVs) and magnetic
fields ($\sim
0.1 - 5 \mu$G) and is collectively
termed as the intra-cluster medium (ICM).
Smaller, less massive ($<10^{14}$ M$_{\odot}$) bound systems of galaxies
that are found around galaxy clusters and in filaments are termed as galaxy groups
\citep[e.g. 3C449 and 3C288][]{2013ApJ...764...83L,2010ApJ...722.1735L}.
Loosely bound complexes of a number of galaxy clusters and groups are termed as
superclusters.

\subsection{Generation and evolution of cosmic rays}
The detectable radio emission from extragalactic sources in and around galaxy clusters is mainly of synchrotron
origin. Therefore it is a direct probe of processes that govern the generation and evolution of relativistic
particles and magnetic fields in the galaxies themselves and in the diffuse media surrounding them.
The variety of radio sources in galaxy clusters can be classified into two broad categories:
\begin{enumerate}[i.]
  \item those associated with individual galaxies in the cluster, and,
  \item those associated with the ICM.
\end{enumerate}

Starbursts (supernovae), active galactic nuclei (AGN) and radio galaxies
belong to class (i). These can be compact radio sources or extended sources, but showing obvious
association
with individual galaxies in the cluster.
The class (ii) sources are diffuse extended sources with sizes typically $\gtrsim100$ kpc and show no obvious
association with individual galaxies.
In this work we will focus mainly on class (ii) sources that are probes of the cosmic ray content and magnetic
 field in the ICM.

 The cosmic rays once produced, will lose energy primarily by synchrotron emission and inverse
 Compton (IC) scattering
 of the Cosmic Microwave Background (CMB) photons.
  The synchrotron losses depend on the energy
 and magnetic field whereas the IC-losses depend on the energy density of the CMB photons and thus,
 will scale with redshift as $(1+z)^{4}$. Relativistic protons of energy 1GeV -1 TeV at cluster cores have
 radiative lifetimes of
 several Gyrs but that of the relativistic electrons are about 0.01 - 0.1 Gyrs.
 The distances over which the cosmic rays can travel within
 their radiative lifetimes is important to understand the observed source sizes.
 The dispersal of cosmic rays from their source into the ICM depends on
 the diffusivity of the ICM. The diffusion time, $\tau_{diff}$ taken by cosmic rays to diffuse to distances
 of Mpc assuming an optimistic spatial diffusion coefficient is several Gyrs \citep{bru14}. This implies that
 cosmic rays once produced will be confined to the cluster and need to be produced $\it in-situ$ in the ICM in the case
 of sources of sizes of 100s of kpc.

  The primary models for the in-situ
  generation of cosmic ray electrons (CRes) are based on (re-)acceleration of electrons via shocks and turbulence and the
  secondary models are based on hadronic collisions \citep[see][for a review]{bru14}. The secondary models
  predict a population of cosmic ray protons (CRp) to accumulate in clusters over its formation that results in
  relativistic electrons via the collisions of CRps and thermal protons \citep[e.g.][]{den80,bla99}.
  An associated gamma ray flux is
  expected but has not been detected so far; stringent upper limits exist based on the Fermi Gamma Ray observatory
  \citep[e.g.][]{ack10,bru12,2014ApJ...787...18A}. In the primary models, shocks in the ICM and turbulence are
  the drivers behind the acceleration of particles and thus are invoked in merging galaxy clusters.
 Radio observations provide the means to distinguish between the roles of these processes in the
 generation of synchrotron emission from the ICM.

\begin{figure}
\centering
  \includegraphics[height=6 cm]{macs0417_halo.pdf}
 \includegraphics[height=6 cm]{a3376_dr.pdf}
   \includegraphics[height=6 cm]{phoenix.pdf}
 \caption{Examples of diffuse radio emission in clusters discussed in this chapter. The X-ray images are
 shown in colour scale and radio images in white contours are overlaid.
 Top left: Radio halo in the cluster MACS0417.5-1154. Image adapted from \citep{2011JApA...32..529D}. Top right:
 Double radio relics in the cluster A3376. Image adapted from \citep{kal12}. Bottom: Radio mini-halo in
 the Phoenix cluster. Red contours show the X-ray emission. Image adapted from \citep{2014ApJ...786L..17V}.
 \label{halorelic}}
\end{figure}

\section {Diffuse synchrotron radio emission from the ICM}
\label{diffuse-synch}
 Cluster-wide non-thermal radio emission
has been a topic of study for nearly half a century since its discovery in
the Coma cluster \citep{1959Natur.183.1663L,1970MNRAS.151....1W}.
Over the last few decades, a large number of galaxy clusters were imaged at radio
wavelengths ($20 - 200$ cm) using a variety of synthesis radio telescopes like the Very Large
Array (VLA), the Westerbork Synthesis Radio Telescope (WSRT) and the Giant Metrewave
Radio Telescope (GMRT). A large variety in the size, morphology and spectrum of these sources
has been found. Based on the properties of the radio sources and the host cluster,
the sources have been classified into three
\footnote{A fourth class of diffuse radio emission are the so-called ``radio phoenixes'' which are smaller scale sources
that have been proposed to be fading and/or re-accelerated remnants of radio galaxy lobes; these are not discussed in
this work.} main classes \citep[e.g.][]{fer12}:
\begin{itemize}
 \item {\it Radio halos} -- extended sources of sizes $\sim$ Mpc, nearly co-spatial with X-ray
 emission from the central regions
 of clusters.
 \item {\it Radio relics} -- elongated, filamentary or sometimes arc-like sources of few hundred to $1-2$ Mpc on
 the longer sides, found at the peripheries of clusters.
 \item {\it Radio mini-halos} -- extended sources of regular morphologies with sizes  $\sim$100 - 500 kpc, surrounding central
 elliptical galaxies in cool-core clusters.
\end{itemize}
Illustrative examples of these sources are shown in Fig.~\ref{halorelic}.
The common components of the ICM which lead to these sources are the relativistic electrons and magnetic fields.

The radio spectra of these sources are typically described by a power-law, $S_\nu \propto \nu^{-\alpha}$,
where $S_\nu$ is the flux density at frequency $\nu$ and $\alpha$ is the spectral index.
The spectral index, $\alpha$ is related to the injection spectral index, $\delta$ of the electron energy
distribution, $N(E)dE = N_0 E^{-\delta} dE$ through, $\delta= 2\alpha+1$ (see textbooks such as
\citet{2000thas.book.....P} for details). The spectra originating as a power-laws in the case of
standard models of particle acceleration can be affected by the effects of overlapping regions of different
magnetic fields,
age of the electron population, energy losses by other mechanisms such as the IC losses
and continuous or intermittent acceleration mechanism. Radio observations over a large range of
frequencies are required to study the spectral properties of radio halos, relics and mini-halos
and infer the state of the relativistic electron population and magnetic fields. Below we discuss each
of these in detail.

The sizes of several hundreds of kiloparsecs in the case of the radio halos imply the role of in-situ
mechanisms of cosmic ray production
in the ICM. The primary electron model invokes
 re-acceleration of electrons from the thermal pool or fossil mildly relativistic electrons via magneto-hydrodynamic (MHD) turbulence injected by
 cluster mergers \citep{pet01,bru01,pet08,2016MNRAS.tmp..288B}. The secondary or hadronic model invokes
 collisions between relativistic protons and thermal protons for producing
 relativistic electrons in the ICM as secondary products along with associated gamma rays
 \citep[e.g.][]{den80,bla99}.
 Based on the upper limits on the gamma ray fluxes from clusters, simulations show that the
 relativistic electrons produced via hadronic models alone are insufficient
 to explain the radio halos \citep[e.g.][]{don13a} but can contribute to forming what are called `off-state' radio halos
 in low mass clusters and relaxed clusters \citep{bru11,bro11}.

 The radio emission in relics shows another mode of acceleration of mildly relativistic electrons to ultra relativistic energies via acceleration by shocks.
 In the large scale structure there are shocks in the filaments that have Mach numbers of 100s and near cluster peripheries shocks
 of Mach numbers of a few (1.5 -4) are found \citep[]{min00,2003JKAS...36..111K}. Diffusive shock acceleration (DSA) has been
 the proposed model for producing relativistic electrons at the shocks  in sources such
 as the radio relics \citep[e.g.][]{ens98}.

 Mini-halos are diffuse sources around the central dominant galaxy in relaxed clusters.
 The secondary electron model and/or re-acceleration of fossil relativistic electrons by turbulence in the
 cool core produced due to the infall of sub-clusters inducing sloshing motions
 have been considered for producing the relativistic electrons responsible for the mini-halos
 \citep[e.g.][]{git02, pfr04,fuj07,kes10,zuh13}. A connection between cold-fronts and the
 mini-halos has also been found \citep{maz08,hla13,gia14,2014ApJ...795...73G}.
 The connection between the central galaxy and the mini-halo and the role of external interaction
 with the cool-core are open questions being addressed using new radio observations and simulations.

\subsection{Past studies}
\subsubsection{Radio surveys}
The radio observations in the past couple of decades have provided a glimpse of the properties and
occurrence rates of the diffuse radio sources in galaxy clusters.
The initial discoveries of the radio halos and relics came mainly from the inspection of
all sky radio surveys such as the NRAO VLA Sky Survey (NVSS,\citet{con98}). It is a survey at 1.4 GHz
carried out using the VLA in D configuration (27 antennas in 1 km$^2$ area)
providing images of the sky with rms sensitivity of 0.45 mJy beam$^{-1}$ where beam$=45''\times45''$.
A number of radio halos and relics in clusters at redshifts $< 0.2$ were discovered
using NVSS and subsequently confirmed with deep follow-up observations
 \citep[e.g.][]{gio99,bag02}.

The low surface brightnesses, $\sim 0.2 - 1\mu$Jy arcsec$^{-2}$ at 1.4 GHz of
radio halos, relics and mini-halos and their extents of several arcminutes to a degree
make them a challenge for imaging with radio telescopes. Aperture synthesis radio telescopes
require a combination of short and long baselines to effectively image the extended sources
and to separate out the contamination by discrete compact sources. A low frequency aperture synthesis telescope
 providing the necessary combination of short and long baselines with sufficient sensitivity
to detect faint structures is ideal to carry out tailored surveys of galaxy clusters.

In the past decade systematic surveys of galaxy clusters at low radio frequencies ($<$GHz) have been taken up
mainly with the GMRT due to its suitable configuration and sensitivity to extended
emission. The ``GMRT Radio Halo Survey'' (GRHS) and its extension, the
``Extended GMRT Radio Halo Survey'' carried out at 610 MHz, are a systematic deep radio survey
of 64 most X-ray luminous ($L_{\mathrm{X}[0.1-2.4\mathrm{keV}]}>5\times10^{44}$ erg s$^{-1}$) galaxy clusters in
the redshift range 0.2 - 0.4. In the GRHS+EGRHS about sample $22\%$ galaxy clusters
contain radio halos, $16\%$
contain mini-halos and $5\%$ contain radio relics \citep{ven07,ven08,kal13,kal15}.
Moreover, the upper limits on the non-detections have showed that
there is a bi-modality in the clusters such that the detections and non-detections are well separated implying
``radio bright'' and ``radio quiet'' \footnote{This terminology is not connected in any way to the one
used in the context of radio galaxies.} clusters in the $P_{1.4\mathrm{GHz}}- L_X$ plane
. Apart from X-ray flux-limited samples of galaxy clusters that have been
explored so far, with the telescopes
such as the Planck, the South Pole Telescope and the Atacama Cosmology Telescope that detect clusters using the
Sunyaev- Ze'ldovich effect, mass limited samples can now be explored.
Radio surveys of complete mass limited samples are ongoing and will provide results in the coming
years \citep{bas12,cuc15,bon15}.

 \subsubsection{Radio halos and relics}
 The observations of radio halos and relics provide the constraints for the
 particle acceleration mechanisms.
 The VLA in C and D configurations, the Westerbork Synthesis Radio Telescope (WSRT) and the
 GMRT have provided the most sensitive measurements of the diffuse radio emission in
 galaxy clusters in the last two decades. Spectral index distribution across the extents of radio halos is
 essential to trace the in-situ acceleration mechanisms and the ageing of the electrons. For this measurement,
 matched arrays at multiple frequencies are needed and were achieved using a combination of telescopes.
 The first spectral index maps of radio halos were made with the VLA and the WSRT \citep[e.g.][]{gio93,fer04}.
 A spectral index study of the radio halo and relic in the cluster A2256 was carried out with a combination
 of the GMRT at 150 MHz, the WSRT at 350 MHz and the VLA at 1400 MHz \citep{kal10}. A spectral steepening
 in the halo at lower frequencies was found in the above observations for the first time and was interpreted in terms of the
 two epochs of particle acceleration driven by two mergers. Deeper studies with the Karl G. Jansky VLA (JVLA)
 have further shed light on the spectral properties of the radio relics \citep{owe14,tra15}.
 The follow-up of MACS
 (Massive Cluster Survey,\citep{ebe10}) clusters with the GMRT have led to the discovery of a halos, relics and mini-halos in couple of
 clusters and a number of other diffuse sources \citep[][]
 {2011JApA...32..529D, 2013A&A...557A.117P,2015sf2a.conf..247P,2016arXiv160802796P}.
 The MACS clusters have also been observed at 2 - 24 GHz with the Australia Telescope Compact Array (ATCA) to study the
 non-thermal and thermal pressures using diffuse emission and the Sunyaev Zel'dovich effect (SZE) \citep{2016Ap&SS.361..255M}.

 The SZE has emerged as a promising probe of discovering new clusters
 in the past few years. The Planck satellite, the South Pole Telescope and the Atacama Cosmology Telescope
 have all led to discoveries of new clusters \citep{2011A&A...536A...8P,2014A&A...571A..29P,2013ApJ...763..127R,2015ApJ...803...79L}.
 The first system of radio halo and relic was discovered in a massive new Planck cluster by \citep{bag11} and
 were followed by discoveries in other clusters \citep[e.g.][]{2013ApJ...766...18G,bon15}. These newly discovered clusters
 have flatter entropy profiles at the cores and are more likely to be disturbed
 given the fact that these were missed in the X-ray flux limited catalogues due to their more disturbed morphology.
 Thus a search for new radio halos and relics in these clusters is on and is furthering the understanding of the
 role of mass and the dynamical state of the cluster in the generation of radio halos and relics.

 Spectral and polarization studies of relics are essential to distinguish between the models for their origin.
 The prototype of cluster peripheral double relics in the cluster A3376 were discovered and proposed to be
 the signatures of cluster merger shocks \citep{bag06}. The spectral and polarization study of the A3376 double radio
 relics led to the observational evidence of its connection to merger shocks \citep{kal12}. The low frequency GMRT
 observations have been crucial in the discoveries of new radio relics
 \citep{wee10,wee11b,2015MNRAS.453.3483D} and
 radio halos \citep[e.g.][]{2013ApJ...766...18G,2014ApJ...781L..32V,2015sf2a.conf..247P}.
 The first among the class of ``ultra-steep spectrum'' radio halos predicted by the turbulent re-acceleration model
 was found in the cluster A520 using the GMRT \citep{bru08}.

 \begin{figure}
\centering
   \includegraphics[height=8 cm]{Zwcl_relic.pdf}
 \caption{Peculiar radio relics found  in  the filamentary merging cluster
ZWCL 2341.1+0000 \citep{bag02,wee09}.
Left panel shows the  radio emission  at
610 MHz from  GMRT  (solid contours),   smoothed to
a circular beam of $15''$  to better show the diffuse radio emission.
X-ray emission distribution  from  XMM-Newton observations
is shown in the background.  Dashed contours show the galaxy iso-density
contours from  Sloan Digitized Sky Survey.  The  SDSS colour image of  cluster ZwCl 2341.1+0000
is shown on the  right panel.
 \label{zwcl}}
\end{figure}

 \citet{bag02} discovered the diffuse radio emission associated in a complex system of merging
groups of galaxies ZWCl 2341.1+0000 in 1.4 GHz NVSS survey, and concluded that this emission was the first
evidence of cosmic-ray particle acceleration taking place at magnetized cosmic shocks in a highly filamentary
environment that is likely in the process of ongoing structure formation.
 In recent years more observations of this unusual and highly filamentary merging
 structure (Fig.~\ref{zwcl}) and a few other systems have revealed some intriguing details (discussed below)
 which brought to light unusual
 aspects of particle acceleration and radio halo and relic formation in elongated,
 filamentary structures:
\begin{enumerate}[a.]
\item The unusually flat radio spectra of the peripheral double relics ($\alpha < 0.5$)
implies high Mach number for the shocks, in contradiction with Mach number estimated from
X-ray observations \citep{bag02,wee09,ogr14}.
\item It is suggested that relics and radio halo in
ZWCl 2341.1+0000 highlight the shortcomings or failure of DSA theory in explaining
the particle injection spectrum in low mass, less energetic filamentary structures
of the cosmic-web \citep{ogr14}. Possibly our understanding of the origin of radio relics is
incomplete, and that non-linear effects are required to explain particle acceleration
at weak shocks.
\item If radio relics result from particle (re-)acceleration at shock fronts, then this
shock should span the whole length of the radio relic it traces. Yet in ZWCL 2341.1+000,
this expectation is not met, where the SE shock front was found to subtend an arc that
is only about a third of the length of the arc subtended by the radio relic; the result
was confirmed with a confidence level of $\sim90\%$ by \citep{ogr14}.  Again
this result is at odds with the standard DSA theory and needs more investigation with deeper
radio observations and modeling.
 \end{enumerate}

 The GMRT observations at multiple low frequency bands have been used to distinguish between merger shock related
 relics and adiabatically compressed lobes of radio galaxies.
 The adiabatic compression model proposed by \citet{ens01} was used to model the spectra of the diffuse emission in A754
 and the relics of double radio galaxies
 \citep{2009ApJ...698L.163D,kal09}. In a multi-wavelength study of radio relics A4038, A1664 and A786, it
 was found that these are relics not associated with shocks but are adiabatically compressed or fading remnants of radio galaxy lobes \citep{kaldwa12}. The GMRT low frequency observations revealed that the radio relic in A4038 is extended to
 over 100 kpc and what was seen earlier from observations at frequencies 1.4 GHz was only the brightest portion.

 \subsubsection{Mini-halos}
 Radio mini-halos are diffuse sources, typically of sizes 100 - 500 kpc that surround the
 central galaxies in cool-core clusters. The central galaxy always has associated compact source
 at its centre but is not connected to the surrounding diffuse mini-halo with jets but may have a
  role in injecting the seed relativistic electrons \citep[e.g.][]{gia14}.
 The secondary electrons due to hadronic collisions may play a role in generating the seed electrons that
 form the mini-halo but are shown to be insufficient to power the mini-halo
 \citep[][]{zuh14}. It has been proposed that the MHD
 turbulence in the cool-core, generated via cooling flow or sloshing cores can lead to re-acceleration of relativistic
 electrons \citep[e.g.][]{git02,maz08}.

 As of now the number count of mini-halos is still limited to about 22 \citep[][Pandey-Pommier et al. 2016, submitted]{gia14}.
 About $50\%$ of the cool-core subsample of the clusters in the Extended GMRT Radio Halo Survey were
 found to host a mini-halo and a scaling between their radio power and
 the X-ray luminosity was explored \citep{kal13}. The cooling at the centres and the mini-halos
 may be connected through scaling relations, but these have not been established due to
 the lack of statistical samples \citep[e.g.][]{bravi16}.

 Low mass clusters have not been surveyed to search for mini-halos; however there are cases such as the
 diffuse mini-halo like radio source in the cluster MRC0116+111 which may be remnants of the radio
 mode activity of the central galaxy \citep[][]{2009MNRAS.399..601B}.

 \subsection{Simulations}
Cosmological simulations using
computations performed with the grid-based, adaptive mesh refinement hydrodynamical code {\it ENZO} show
that turbulence in clusters can be sustained on timescales exceeding a Gyr \citep{pau11}.
In the same work it was proposed that the breaking of shocks (seen as high temperature
structures in the simulation slices) at inflowing filaments around the cluster can produce notches in the radio relics
(Fig.~\ref{paul}). Simulations
including magnetic field evolution along with the structure formation and radiative cooling can provide
predictions for the radio emission from the large scale structure based on the recipes for production of
relativistic electrons \citep[][]{2007MNRAS.375...77H, don13a,vaz14,2015A&A...580A.119V}.
It has been shown that a saturation of magnetisation can be achieved in a fully turbulent medium and there
is near equipartition between
the magnetic field and kinetic energy densities \citep[e. g.][]{sub06,2012MNRAS.423.2781I}. Magnetic field
can be evolved in the simulation using the estimate of turbulence and a scaling between turbulent and magnetic energies.
This has been implemented by Paul et al. (2016, in prep.) in the case of Coma and shows agreement with the observed magnetic field profiles \citep{2010A&A...513A..30B}
based on Faraday rotation of background sources. Radio mini-halos due to electron reacceleration by minor merger driven
turbulence has been simulated by \citet{zuh13}. Implementation of diffusive shock acceleration and turbulent acceleration
to accelerate cosmic rays is being used to predict synchrotron emission that will be observable with the SKA.
Predictions by Paul et al. (2016, in prep.) indicate that the estimate of surface brightness at 1.4 GHz with a beam of
$20''$ is about $10^{-8}$Jy beam$^{-1}$ from the filaments if only turbulent reacceleration is considered
and in the range $10^{-6}$ Jy beam$^{-1}$ if DSA is also included and denser regions such as groups and cluster
outskirts are considered. The uncertainties such as efficiency of turbulent reacceleration and magnetization in the large scale structure remain and will be constrained by deeper observations that will be made possible by the SKA.

 \begin{figure}
\centering
 \includegraphics[width=\textwidth]{p11fig.pdf}
 \caption{Evolution of the shock in temperature in a simulation by \citet{pau11}, as seen from slices in three different planes of the computational volume. The panels refer to z = 0.1 and to slices
perpendicular to the x-axis (left), to the y-axis (central), and to the z-axis (right), respectively. Each panel has a size of $7.7\times7.7$ Mpc $h^{-1}$ and is cut along the center of mass of the system.\label{paul}}
\end{figure}

\subsection{Prospects for the SKA}
In this section we discuss the numerous possibilities of studying diffuse radio emission from galaxy clusters
opened by SKA, thanks to its unprecedented sensitivity.
\subsubsection{Deep continuum and polarization imaging of halos, mini-halos and relics}
Radio halos, relics and mini-halos in general have low surface brightness ($\sim1\mu$Jy arcsec$^{-2}$ at 1.4 GHz)
and among these, radio halos have the lowest brightness levels. The average surface brightness of the known radio halos
at 1.4 GHz is $\sim0.25\mu$Jy arcsec$^{-2}$ \citep[inferred using the data in][]{fer12}. The
SKA1-low\,\, will achieve a resolution of $7''\times7''$ at 110 MHz (Table ~\ref{skasens}).
In order to map the extended sources,
the images are produced at a lower resolution than the best offered by the telescope configuration.
Therefore we assume a canonical resolution of $10''\times10''$ for multi-wavelength observations of
diffuse radio sources with the
SKA1-low\,\, and SKA1-mid\,\, and discuss the predictions.

The currently prevalent models of turbulent re-acceleration for radio halos predict that the spectra
change from a power-law to an exponential decay beyond a certain critical frequency \citep{bru14}.
Assuming the critical frequency to be 1.4 GHz, the spectrum
corresponding to the mean value of surface brightnesses of known halos
is plotted in Fig.~\ref{rhpred}. The rms confusion at cm wavelengths assuming a Gaussian
beam is approximated as \citep{2002ASPC..278..155C},
\begin{equation}
 \bigg(\frac{\sigma_c}{\mathrm{mJy \,\,beam}^{-1}}\bigg) \approx 0.2 \,\,\bigg(\frac{\nu}{\mathrm{GHz}}\bigg)^{-0.7} \bigg(\frac{\theta_{b}}{\mathrm{arcmin}}\bigg)^2.
\end{equation}
The expected rms confusion at the four frequencies of 0.15, 0.6, 1.4 and 5 GHz (Fig.~\ref{rhpred}) are
shown in comparison to the radio halo spectra.
It is clear from this figure that most of
the known halos can be imaged up to 5 GHz if the cut-off frequency is
$\sim$ 1.4 GHz, but, only up to 2 GHz, if the cut-off occurs earlier.
The surface brightnesses of diffuse sources are not uniform. The profiles of radio halos
show that the central regions are the brightest with a gradual fall towards the edges.
With SKA1-low\,\, and SKA1-mid\,\,, the known radio halos, relics and mini-halos can be imaged to a factor of a few
deeper. The profiles of the radio halos in the outskirts of the clusters will provide clues to the underlying
cosmic ray and magnetic field profile with implications to the proposed models for the generation of
radio halos. It will be possible to reliably map spectral indices over the extent of the radio halos.
This will lead to constraints on the in-situ acceleration mechanisms at work in the cluster.
The case of radio halos discussed here is an illustration of the weakest of the diffuse radio sources in clusters.
Radio relics and mini-halos being a few times brighter in surface brightness will be imaged in detail
 leading clues to their origin and evolution.
\begin{figure}
\centering
 \includegraphics[width=15 cm]{spectra_radiohalo_2.pdf}
 \caption{Surface brightness of radio halos as a function of frequency.
 The lines indicate the expected spectra for radio halos that are
 a combination of a power-law and an exponential decay. The critical frequency
 where the exponential decay starts is 1.4 GHz (solid lines) and 0.6 GHz (dashed lines), respectively.
The three sets of spectra are for three different
surface brightness values, 10, 25 and 50 $\mu$Jy / 100 arcsec$^{2}$ for the
halos at 1.4 GHz.
The short horizontal lines labelled a, b, c and d indicate the expected confusion limits
($\mu$Jy / 100 arcsec$^{2}$) at the frequencies $0.15, 0.6, 1.4$ and $5$ GHz, respectively. \label{rhpred}}
\end{figure}

Furthermore, polarization is a direct probe of the magnetic field
in the plane of the sky and complements the line of sight magnetic field estimated via Faraday rotation of the
plane of
polarization of background sources.
Through polarization observations coherence lengths of magnetic field can be inferred
and that is used to refine the simulations.
Radio halos typically have low polarized emission fraction $<5\%$ or so \citep{fer12}.
Polarization detection claimed in the radio halo of the cluster A2255 but it is likely due to
polarized filament in the periphery of the cluster seen projected on the cluster
\citep[][]{2005A&A...430L...5G, 2011A&A...525A.104P}. Radio mini-halos are at cluster centres and thus
depolarization is expected due to the ICM and hence little is known about their polarization properties.
Radio relics are known to be polarized up to $10-30\%$, as expected based on their origin in shock acceleration
\citep[see][for reviews]{fer12,bru14}. SKA1-mid\,\, sensitivities will allow to probe the polarization
properties of these sources to much deeper
levels than currently possible and provide important constraints on magnetic fields in clusters of galaxies.

\subsubsection{Constraining high frequency spectra of radio halos, relics and mini-halos}
The spectra of radio halos, relics and mini-halos are important to constrain models proposed to
explain them. The turbulent re-acceleration model predicts that the spectra will steepen exponentially
beyond a break frequency decided by the turbulent energy budget in the cluster \citep{cas05,cas06}.
A handful of sources have been imaged at more than three frequency bands below 1 GHz \citep{fer12}
and at frequencies higher than a GHz,
the spectra are largely unknown. Recently two relics were imaged in the frequency range 0.15 - 30 GHz
using a number of radio telescopes and its spectrum shows departure from the expectations
from the DSA model \citep{2016MNRAS.455.2402S} but theoretical
works argue that DSA can explain it under certain condition of a shock passing through a cloud of fossil population of
relativistic electrons \citep{2016arXiv160203278K}.
It is important to probe the spectra of these diffuse sources at $>$GHz frequencies to
locate the spectral breaks in them and to test the models.

Characterisation of galaxy clusters at $>10$ GHz is hampered by the presence of the SZE.
The distortion of the spectrum of the CMB spectrum due to
inverse Compton scattering of the CMB photons by the thermal electrons in the ICM is known as the
SZE \citep{1972CoASP...4..173S}. At frequencies in the range of tens of GHz,
the CMB produces a negative signal that can be mixed with the positive radio emission due to radio halos.
It is possible to model the signal due to SZE as it has a $\nu^{2}$ dependence and study the radio emission.
Studies with ATCA at frequencies 9 and 18 GHz have shown that radio halos (also relics) such as that in the Bullet cluster
can be detected, though mixed with the SZE \citep{2010arXiv1005.1394M,2011JApA...32..541M,2016Ap&SS.361..255M}.

Observations at matched resolution at high and low frequencies are needed to accurately study the radio halos and
the SZE at GHz frequencies. We discuss the expectations for SKA1-mid\,\, using the Fig.~\ref{rhpred}.
It can be seen that most of
the known halos can be imaged up to 5 GHz if the cut-off frequency is
$\sim$ 1.4 GHz, but, only up to 2 GHz, if the cut-off occurs at lower frequencies.
However the spectra above 2 GHz for the radio halos, relics and mini-halos are largely unknown except in a few cases
and presents an obvious niche for new observations.

\subsubsection{Search for new radio halos, relics and mini-halos}
The all-sky continuum surveys and targeted surveys of complete samples of clusters
with the SKA will open windows to discover 100s to 1000s of new radio halos, relics and mini-halos.
The statistical occurrence of the diffuse radio sources is critical to study their origin and evolution in the context
of the evolution of the clusters themselves. Current telescopes have allowed a limited number of statistical studies
owing to the long observations needed to image with high sensitivity \citep{ven07,ven08,kal13,kal15,cuc15,bon15}.

The prospects with the SKA to search for such sources in blind surveys and with targeted observations are promising.
From Fig.~\ref{rhpred} it is seen that SKA1-low\,\, will detect new radio halos as it will
reach much better sensitivities than the current instruments.
Based on the turbulent acceleration models, it has been predicted that
about 2600 new radio halos will be discovered in a survey that can reach
rms 20$\mu$Jy beam$^{-1}$ with a beam $\sim10''$ at 120 MHz \citep{2015aska.confE..73C}.
From the studies of the known radio halos it has been  inferred that about $58\%$ of the flux density of the radio halo is contained within half its radius
\citep{bru07}. A minimum detectable flux
 density of a radio halo, $f_{min}$ can be inferred if it is assumed that a radio halo is detectable when the integrated flux
 density within half its size gives a signal to noise ratio, $\xi$ \citep{2015aska.confE..73C}. It means that
 $f_{min}(<0.5\theta_H) \simeq \xi \sqrt{N_b} F_{rms}$, where $N_b$ is the number of independent beams within $0.5\theta_H$.
 It is found that,
 \begin{equation}
  f_{min} \simeq 1.43 \times 10^{-3} \xi \bigg(\frac{\mathrm{F}_\mathrm{rms}}{10\mu\mathrm{Jy}} \bigg) \bigg(\frac{10''}{\theta_b} \bigg) \bigg(\frac{\theta_H(z)}{\mathrm{arcsec}} \bigg).
 \end{equation}
The minimum power of radio halo detectable as a function of redshift for the case of $\xi=7.0$ is shown in Fig.~\ref{rhpred2}.
 The redshifts beyond 0.4 are essentially unexplored and SKA will provide the first glimpse of the properties of
 radio halos at those redshifts. The ``off-state'' of clusters which are below the current GMRT upper limits
 will be detected using the SKA1-low\,\,. This is critical to understand the cosmic ray content of galaxy clusters.

\begin{figure}
\centering
 \includegraphics[width=10cm,angle=-90]{pow_z_ska.pdf}
 \caption{The expected detection thresholds for SKA1-low\,\, in comparison to the known radio halos. Note that
 the power at 110 MHz is shown for SKA1-low\,\,. If it is scaled to power at 1.4 GHz, the expected levels
 are lower by a factor $(0.11/1.4)^{\alpha}$, where $\alpha$ is the spectral index between 0.11 and 1.4
 GHz. The known halos from literature and the GMRT upper limits are from \citet{kal15}.\label{rhpred2}}
\end{figure}

\section{Superclusters and filaments}
\label{scs}
Binary clusters and systems of multiple interacting clusters can be found in
superclusters or as independent systems. Typically such systems may be either
in a stage before they fall into each other or could have undergone the merger
and are oscillating. In both these cases it is interesting to study the
ICM in and around these clusters to probe the dynamics of diffuse matter and
cosmic rays.

Superclusters such as the Shapley supercluster (SSC) are among the nearest systems available for study.
About 28 clusters were identified within a volume of $2.5\times10^{5}$ $h^{-3}$Mpc$^3$ -- that is an over density
 of more than a factor of ten with respect to the mean density of Abell clusters at similar galactic latitudes
 \citep{1989Natur.338..562S}. SSC is also the richest SC in terms of the presence of X-ray emitting clusters
 \citep{1991MNRAS.248..101R}. Dedicated studies of this region in optical, radio and X-rays
 have revealed several sub-structures within this SSC \citep[e.g.][and references therein]{2000MNRAS.314..594V}.
 Recently observations of SSC were carried out with the SKA precursor, Murchison Widefield Array (MWA) with the aim of probing diffuse
 radio emission at cluster and inter-cluster scales (Kale et al. 2016, in prep.).

 The SKA1-low\,\, opens up the possibility of probing inter-cluster scale radio sources at even better
 sensitivity than possible with the current MWA. Apart from SSC other binary clusters and superclusters will
 be of interest to probe the acceleration of cosmic rays and magnetic fields in these regions.
 Targets of interest can be filaments between interacting clusters detected by Planck \citep{2013A&A...550A.134P}.

Apart from the denser structures like the clusters of galaxies and galaxy groups,
there are filaments in which a large fraction of the galaxies in the Universe reside.
Filaments also contain a large reservoir of inter-galactic medium called the
warm hot inter-galactic medium (WHIM) with temperatures in the range $10^{5} - 10^{7}$ K
that has been processed by accretion shocks and is extremely difficult to detect
in most wavelength bands. Radio bands stand a chance of detecting it if the shocks
 accelerate electrons. A detection will be able to probe the cosmic
rays and magnetic fields in the filaments. Flux densities of $\sim 0.12 \mu$Jy at a redshift
of 0.15 at 150 MHz have been predicted assuming that primary electrons are accelerated
at cosmological shock waves \citep{2012MNRAS.423.2325A}. A radio detection of filaments has
been predicted in regions where magnetic field is about $\sim$10 -100
nG \citep{2015aska.confE..97V}. Recent MHD simulations using $\emph ENZO$ have predicted that
a non-detection with the SKA can place constraints on the magnetic energy
in the WHIM to be less than $\sim 1\%$ of the thermal energy \citep{2015A&A...580A.119V}.

Thus although it seems difficult to detect, a strong case exists for detections of filaments
 surrounding massive clusters. Recently filaments of temperatures $\sim10^7$ K were detected in X-rays
 around the massive and merging cluster Abell 2744 \citep{2015Natur.528..105E}.
 If detected in radio, these can potentially constrain
 the magnetic field in them.

\section {Tailed radio galaxies as tracers of inter-galactic weather}
\label{head-tail}

\subsection{Previous studies}
`Tailed' radio sources \citep{1968MNRAS.138....1R} are
characterised by a head identified with the optical galaxy
and two trails of FR\,I radio source sweeping back from the head
\citep{1972Natur.237..269M,1973A&A....26..423J}.
These sources are usually found in rich cluster environments,
where jets are understood to have been swept back by the deflecting pressure
of the dense ICM (e.g. Fig.~\ref{headtail}).
Furthermore, the long tails of these galaxies carry the imprint
of relative motion between the non-thermal plasma and the ambient hot gas.
Hence, in the parlance of the field, they reflect the weather conditions of
ICM and the jet dynamics, which allows us to make quantitative statements about
their dynamics and energetics.
Two specific examples of the interaction between radio sources and the ICM are
wide-angle tailed (WAT) and narrow-angle tailed (NAT) radio
sources, where the latter are also addressed as the `head-tail' radio sources.

Recently, a radio study was conducted, using GMRT
for a sample of head-tail radio sources,
concentrating on 3C129, NGC~1265 and IC~310 \citep{2009ASPC..407..157L,2004A&A...420..491L}.
New X-ray observations were proposed for objects which are in poor environments
where temperature
and abundance variations are likely to be more visible in the X-rays \citep{1994AJ....108.1137R}.
When combined with radio data,
these multi-waveband data probe a variety of studies, namely
(i) collimation and surface brightness of the jets \citep{2014MNRAS.437.3405L,2002MNRAS.336..328L},
(ii) radio jet--ICM interaction \citep{2012ASPC..459..155P,2012IJMPS...8..241P},
(iii) infall of tailed radio sources into the cluster,
(iv) details of cluster merger \citep{2011ApJ...743..199D},
(v) gas pressure to compare with equipartition pressure,
(vi) energy losses, particle acceleration, and
(vii) cluster centre ambiguities.
The potential of such observations is also to reveal
details of cluster mergers such as subsonic $/$ transonic bulk flows,
shocks and turbulence.
Fortunately, the jets survive the encounter
with the ICM, with possible shocks leading to the formation of long
tails, that are devoid of the growth of
Kelvin-Helmholtz instabilities \citep{1995ApJ...445...80L}.

\begin{figure}
\centering
  \includegraphics[height=6 cm]{dharam_ds9.pdf}
 \caption{Low frequency, full synthesis GMRT image of head-tail sources in Perseus cluster at 240 MHz. Note the presence of dominant 3C84 radio source and several head-tail radio galaxies, including NGC1265 and IC310.  The field is 4 sq. deg, rms noise is 8.1 mJy beam$^{-1}$ and the angular resolution is 9 arcsec.
 \label{headtail}}
\end{figure}

\subsection{Prospects for the SKA}

To illustrate in detail, let us consider two specific science cases related to jets of radio
galaxies in cluster environment,
(i) is deceleration of jets in these objects is caused by
internal entrainment or if the mass-load of the jet is external
\citep{2012IJMPS...8..241P,2011ApJ...743...42P}
and
(ii) how does the local ICM play a role in shaping
NAT and WAT galaxies
\citep{1996ApJ...473..651R}.
To answer (i),
observationally the transverse velocity profile of the radio jets
can give clues to understand which of these two processes is more
relevant; if former, no velocity profile across the jet is expected,
whereas in latter case, there would be a velocity profile
with slower layers at the jet boundaries \citep{2002MNRAS.336..328L}.
Next to answer (ii), comparisons between the radio morphologies of
tailed sources in cluster environments and the distribution of
the thermal gas as seen in \textit{Chandra} and \textit{XMM-Newton}
images, indicate that the thermal gas is almost always asymmetric
and aligned towards the direction of the bending \citep{1994ApJ...436...67V}, and many a times
these clusters are undergoing mergers, resulting in large-scale
flows of hot gas owing to the changing gravitational potential \citep{2004MNRAS.351..101K}.
Therefore tailed radio sources in merging clusters
are diagnostics of the ICM weather and of the evolving
gravitational potential resulting from the merger
as compared to (tailed) radio sources in relaxed clusters.
This argument clearly answers the role played by relaxed and merging clusters
in shaping WATs and NATs.

A series of tiered surveys with increasing sensitivity, but
decreasing in areas are planned to be undertaken with SKA phase-1
(SKA-1). Briefly, the 1--2 GHz band of SKA\,1, with 2~arcsec resolution and
2 $\mu$Jy beam$^{-1}$ will detect several orders of more number of
WAT and NAT radio sources
and hence their parent clusters with whom they are associated.
Clearly, at this resolution and depth we will not only
resolve the radio jet in longitudinal direction, but also in
transverse direction and boost our statistical understanding of at least two
specific science cases discussed above.

\subsection{Building Statistics using SKA}

VLA Fiant Images of the Radio Sky at Twenty-cm (FIRST) survey
listed $\sim$384 WAT and NAT radio sources selected from
3000 deg$^2$ of sky. Of these \citep{2001AJ....121.2915B} have confirmed the existence
of 40 clusters with redshifts up to $z \simeq$ 0.9.
To compare these, we next try
to understand number of WATs and NATs likely to be detected
with SKA surveys.
The current deep surveys of smaller parts of the sky such as the
$\sim$4~deg$^2$ of the ATLAS-CDFS (Australia Large Area Survey of
the \textit{Chandra} Deep Field--South) field was performed
using ATCA at 1.4\,GHz \citep{2011PASA...28..215N} with $\sim$11~arcsec resolution
and a depth of 15 $\mu$Jy beam$^{-1}$.  Additionally,
VLA image of the Extended-CDFS, again at 1.4\,GHz with
$\sim$2~arcsec resolution has a depth of 10 $\mu$Jy beam$^{-1}$
\cite{2013ApJS..205...13M}.
Although SKA\,1 survey will be similar to this resolution, it will be
marginally more sensitive to the VLA--Extended-CDFS
\citep[Figure~5,][]{2014AJ....148...75D},
\citep[Figure~1,][]{2015aska.confE.101J}
and \citep{2015IAUS..313..321J}.  The above surveys detected $\sim$3000 radio sources, of which
45 are WAT or NAT radio sources and the rest are extended or
(complex) diffuse or ambiguous \citep{2011JApA...32..491D}.  Extrapolating
from these detections, again using \citep[Figure~1,][]{2015aska.confE.101J},
the SKA level surveys will detect
$\sim$10$^6$ WAT and NAT radio sources.
The all-sky radio continuum survey using SKA\,1
will provide more sensitive data to explore a variety of science goals,
including a huge sample, $\sim$10$^6$ clusters of galaxies containing
WAT and NAT radio sources.  Statistical studies of such large samples
of tailed radio sources will provide insights into both the
internal characteristics of astrophysical jets and the
surrounding ICM.

\section{Summary}

This chapter highlights the scientific problems in the area
of galaxy clusters and the cosmic web that can be effectively
addressed using the Square Kilometer Array.
The outstanding problems that need to be addressed are:
\begin{enumerate}[a.]
\item the production and sustenance of relativistic particles and
magnetic fields that are responsible for the observed diffuse
radio emission on cluster-wide scales,
\item the relative importance of
shocks, turbulent acceleration and hadronic models to the production of
cluster-wide radio emission,
\item the detailed properties of the
intra-cluster medium using cluster radio galaxies as tracers, and
\item the faint radio emission arising in structure formation
shocks (the cosmic web).
\end{enumerate}

An underlying theme in the observational study of clusters and
the cosmic web is the detection of low surface brightness and
extended radio emission over a wide range of frequencies like
0.1 - 10 GHz. SKA, with its long baselines and good short spacing
coverage, will be an ideal instrument to detect these features.
It is expected that SKA will reach detection limits that are
a factor of 10 to 50 lower compared to those of the
existing telescopes.  This improved sensitivity is expected to
discover an order of magnitude larger number of clusters
with faint diffuse radio emission hitherto undetected. These
observations from SKA are expected to revolutionise the field
of clusters and the cosmic web.

\section*{Acknowledgments}
We thank the anonymous referee for providing comments on our paper.
RK and SP acknowledge the support through the DST-INSPIRE Faculty Award.
JB  and  MP gratefully acknowledge generous support from the Indo-French Center
for the Promotion of Advanced Research (Centre Franco-Indien pour la Promotion de la Recherche Avan\'{c}ee)
under programme no. 5204-2. Research in Astronomy at IIT Indore was made possible through a grant by the institute.
We thank the staff of GMRT, who made these observations possible. The GMRT is run by the National Centre for Radio
Astrophysics of the Tata Institute of Fundamental Research.
\bibliographystyle{mn2e}

redpajama_set_name: RedPajamaArXiv


text:
Home > Fiction > Short reads > Men on DV (Domestic Violence) by Kailash Amesur
Men on DV (Domestic Violence) by Kailash Amesur
Non-fiction, Short reads
The book takes you on a journey of hitherto untold truths behind the drama when such fake cases are filed, about how the Law which was made to safeguard all behaves like a jealous mistress.
Women protective laws were made to safeguard the women from age-old oppression, but these laws were made when women were mere house dwellers confined to the four walls of their homes and unable to voice their plights, but as times changed the modern woman of today has achieved equal if not a superior status with the men in their lives, their abilities and responses have also developed multifold.
But the Law hasn't imbibed this change in scenario where the hunted can also become the hunter, and this provides the perfect hotbed for a premeditated conspiracy to exact revenge on a spouse and also to render irrevocable damage to his survival and financial security, the author has given voice to the muted stories which never caught attention in the social dogma that domestic violence is all about women at the hands of men, there has to be a shift, Law has to be inclusive and it's high time that we acknowledge the need to rethink and amend it accordingly so it wouldn't be misused, or the very Law that protects shall become the noose around the necks of the unassuming Innocents.
Read online Men on DV (Domestic Violence) by Kailash Amesur
2 hours of read Perspectives on Law real life stories social justice
The Successful Bible by Johnathan David Goldsky
Business, Non-fiction, Self-developement
Change Starts With Me by Taida Spicer
Memoir, Non-fiction, Self-help
Top 16+ Chilling Short Horror Stories and Collections In Order (2022)
Horror, List, Short reads

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Soul & Sensibilities is a poetic and captivating collection of artworks showcasing an intricate interaction between photography, Chinese brush painting and calligraphy. Marrying the techniques of the conventional mediums seamlessly, each artistic creation tells of a narrative that is uniquely meaningful to each viewer.
This collection is the culmination of a year-long collaboration between avid photographer Kwek Leng Joo and highly regarded master painter Lin Lu Zai. Leng Joo's photos reveal the soul of nature while Lu Zai's strokes and calligraphy add a touch of sensibility. The result is a unique art expression that is much more than the sum of its parts. The moment of realisation that there is another dimension gives this series of artworks its distinguishing persona and impact.
The two created masterpieces through an intuitive and symbiotic understanding of each other's creative expression. The experience expanded the boundaries of their respective mediums, blurring the lines between reality and imagination. For Leng Joo, the difficult task was distilling noteworthy subjects from the ordinary and composing them in befitting frames that would form as backdrops to Lu Zai's finishing touches. For Lu Zai, his creativity and imagination were put to the test as he had to interpret Leng Joo's intent and complement it with suitable calligraphic strokes and paintings. Through this collaboration, Leng Joo and Lu Zai hope to leave behind a legacy that will convey the exquisiteness of nature to more people, and enrich future generations' appreciation for the natural environment.


text:
AM ONLY Presents: "The Cookout" A new weekly radio show on Sirius XM
AM Only Presents: "The Cookout," a new radio show on SiriusXM's Electric Area channel. The idea behind The Cookout is to provide AM Only artists a platform to expose their personalities, music and curation abilities while also providing SiriusXM a unique, new tastemaking medium.
The Cookout launches on Tuesday, July 28 at 6PM PT / 9PM ET with a special Rudimental B2B Gorgon City DJ set. In the coming weeks, listeners of The Cookout will be treated to sets from Jauz (July 5), Just Blaze (July 12) and AC Slater Presents Night Bass (July 19), to name a few.
Each artist featured on The Cookout becomes a resident "chef" for the week by offering a menu of sounds to dance music fans – some sounds familiar, some more obscure. Musically, the freedom lies within each artist. The menu changes each week and adapts fan tastes while encouraging listeners to try something new.
"We are excited to get in the kitchen with AM Only to carry this new show of the very best new Electronic Dance Music sounds from young talent. There will be much to love and nothing predictable about the play list. SiriusXM has built its Electronic Dance Music reputation on playing host to the new and the next, and we are doing that again with The Cookout," said Geronimo, VP of Dance Programming, SiriusXM.
"We are very excited about the launch of The Cookout. For our tour marketing team, we are always looking for new platforms to reach electronic music's core audience. SiriusXM has built a very loyal listener base and it was a perfect fit to collaborate with them to develop a show that allows our artists another vertical to launch their tours or help them reach that audience with their new single, EP or album," said Sam Alpert, VP, Marketing, Paradigm Talent Agency and AM Only
As SiriusXM is a subscription service, artists are free to express themselves and play whatever they like during the show. Be sure to tune in for up-to-date news about weekly "chefs."


text:
Don Jr. Opens Up About The Terror Attack Against His Family
Benny Johnson Columnist, Viral Politics
October 26, 2018 4:01 PM ET
President Donald Trump's eldest son, Donald Trump Jr, received an envelope containing a suspicious white powder last February.
Don Jr.'s wife at the time, Vanessa Trump, and members of her staff were hospitalized out of caution after coming in contact with the envelope. The white powder turned out to be harmless, but a letter included in the package read, "You're an awful person and now you get what you deserve."
NEW YORK, NY – NOVEMBER 09: Republican president-elect Donald Trump and his son Donald Trump Jr. embrace after delivering his acceptance speech at the New York Hilton Midtown in the early morning hours of November 9, 2016 in New York City. Donald Trump defeated Democratic presidential nominee Hillary Clinton to become the 45th president of the United States. (Photo by Mark Wilson/Getty Images)
The note continued, "I am surprised that your father lets you speak on TV. You make the family idiot, Eric, look smart. This is the reason why people hate you, so you are getting what you deserve. So shut the f**k UP!"
The man responsible for these mailings — 24-year-old Daniel Frisiello of Beverly, Massachusetts — was a leftist who donated to leftist causes. Frisiello has pleaded guilty, according to the Hill:
The Department of Justice (DOJ) announced that Daniel Frisiello, 25, pleaded guilty to 13 counts of mailing a threat to injure, and six counts of false information and hoaxes. He has been under house arrest since he was charged in March, and will be sentenced in January.
NEW YORK, NY – APRIL 05: Vanessa Trump and Donald Trump Jr. attend the 9th Annual "Dressed To Kilt" charity fashion show at Hammerstein Ballroom on April 5, 2011 in New York City. (Photo by Andrew H. Walker/Getty Images)
This week, suspected pipe bombs were delivered to the CNN offices in Manhattan, the homes of former presidents Barack Obama and Bill Clinton and billionaire George Soros.
Other suspicious items were sent to the offices of Democratic. Rep Maxine Waters and former Attorney General Eric Holder, Cory Booker and James Clapper, but were intercepted.
In light of the recent scourge of mail bombs being sent, Don Jr. opened up about the experience getting terrorized himself and the double standard in the media for coverage of conservatives vs. liberals being victims of violence.
Tags : barack obama cnn donald trump donald trump jr
Benny Johnson


text:
District kicks off second semester with mid-year convocation
By NIKKI SMITH,
At the Petal School District mid-year convocation, the district announced both the overall Petal Teacher and Administrator of the Year.
Lori Johnson, a teacher at Petal Upper Elementary School, was named Petal Teacher of the Year. This is the second year that an upper elementary school teacher claimed the title.
Margaret Tynes was named Administrator of the Year.
Director of the Center for Families and Children Dede Smith introduced the teachers of the year.
"There are lots of superstars in our district," she said. "You're all worthy."
She welcomed Johnson to the stage to claim the title of District Teacher of the Year.
"I feel like I'm in a room full of giants," she said. "You all have poured into my life over the years."
The Brandon native teaches sixth-grade English Language Arts and Social Studies. She has worked for the Petal School District for all 15 of her years in education.
Johnson said it is the guidance from teachers and administrators like Lawrie Wallace, Emily Branch, Dede Smith and Gloria Wyatt, who have mentored her, that means the most.
Others who Johnson said have encouraged and taught her over the years include Robin Atwood, director of the South Mississippi Writing Project and World Class Teaching Program at USM; educational authors like Kylene Beers, Kelly Gallagher, Rose Cappelli, Lynne Dorfman, Timothy Rasinski, Joseph Harris and many others.
Johnson earned her Associate of Arts from Jones County Junior College. She received her bachelor's degree in elementary education from The University of Southern Mississippi and Master of Education in Mild and Moderate Disabilities from William Carey University.
Tynes, the 2017-18 Administrator of the Year, wears a number of hats in her position in the school administration office, but the one she wears most proudly is that of chief cheerleader for the school district.
As the mother of three Petal High graduates (Paul, Daniel and Charley), Tynes knows how important Panther Pride is to the community and she serves as a conduit for those both in and out of the district who wish to see it succeed.
Dillon said she typically tosses them in the trash when she receives nominations for her for the award. He said they received many nominations this year, and that Tynes is nominated each year.
Tynes was surprised, as she had made the powerpoint announcing the recipient of the award and her name was not what was printed on it that morning.
"She is very deserving and has a big heart for people," Dillon said.
At the beginning of the convocation, Dr. Superintendent Matt Dillon, who recently recovered from the flu, took the stage to welcome faculty, staff and administrators back from Christmas break.
"We are halfway to the finish line," he said. "Over the break, I had some time of reflection looking back on 2017."
Dillon said he took some time to think back over the tornado; snow day; awards given to many people in the district; the fact that the Petal School District was named No. 1 school district in the state of Mississippi and the success of the arts, academics and athletics over the past year.
He also had some positive words and encouragement for everyone as the second half of the 2017-18 school year begins.
"Seize every opportunity to make a positive difference," Dillon said. "Despite what season of life, when we come together, great things will happen. Great things are ahead for Petal School District, thanks to our secret weapon: our faculty and staff. I'm proud of our district and proud of the direction we're going."
Steve Gilliland, an award-winning speaker and comedian, said that being a teacher is not a career, but a calling. He asked each person to consider what five people have made the biggest impacts in their lives and to aim to be one of those people for someone else.
As the Petal School District faculty, staff and administrators head into another semester, Gilliland told them to prepare hard and finish easy.


text:
Q: Visual Studio 2022 Preview "MEF Service Broker Package" package not found I installed VS2022, but getting this error
I tried solutions like deleting the ComponentModelCahce folder, or 'devenv /updateconfiguration' and 'devenv.exe /clearcache', but not worked.
Thanks for help.

A: I've just had identical issue, i.e. different messages like the below one were popping-up:

The 'Microsoft.VisualStudio.ProjectSystem.VS.Implementation.Package.ProjectPackage' package did not load correctly.

ActivityLog.xml showed the following message:

SetSite failed for package [MEF Service Broker Package]Source:
'mscorlib' Description: Illegal characters in
path.
System.ArgumentException: Illegal characters in
path.
   at System.IO.Path.NewNormalizePath(String
path, Int32 maxPathLength, Boolean expandShortPaths)

at System.IO.Path.NormalizePath(String path, Boolean fullCheck, Int32
maxPathLength, Boolean expandShortPaths)
   at
System.IO.Path.GetFullPathInternal(String path)
   at
System.IO.DirectoryInfo.Init(String path, Boolean
checkHost)

The following steps helped me:

*

*Uninstall Visual Studio

*Restart Windows

*Remove C:\Users\(your_username)\AppData\Local\Microsoft\Visual Studio

*Remove C:\Users\(your_username)\AppData\Roaming\Microsoft\Visual Studio

*Install Visual Studio

redpajama_set_name: RedPajamaStackExchange


Luigi Rosselli Architects have applied a lot of thought to grey matter over the years: off-form concrete, cement toppings, polished concrete, precast, glass reinforced; concrete is a material of many forms. In-situ cast off-form concrete combines a structural solution with a lasting finish, textured or smooth, coloured dark or light. Using weathered timbers, corrugated iron and embossed patterns or shapes in the formwork provide highly textured and expressive finishes.
While the natural Portland Cement colour is preferred, off-white cements and concrete dyes can add drama. Black and white aggregates can be added to floor slabs, revealed when the floor is polished to a very resilient, hardwearing sheen. Waxing the surface softens the tactile quality.
Glass reinforced concrete (GRC) is increasingly being used to minimise the carbon footprint and energy impact by reducing the amount of material involved. One of the primary motivations for carefully using concrete is to provide a building with few maintenance requirements and a structure that is designed to spread its high production energy cost over centuries.


text:
Why Living in Orange County Is Better Than Los Angeles
By Taylor Hamby Published On 01/22/2016
Flickr/Kwong Yee Cheng
Let's be honest: Orange County basically lives in LA's shadow and often gets picked on, like the tween forced to sit at the kid's table during Thanksgiving. But you know what, irrational haters? Orange County stands just fine on its own, thank you very much. And while the OC'll always live in LA's smog, we don't live in their shadow -- and here's why:
Better beaches
Let's be realistic here: all Southern Californian beaches are comparatively polluted. But between the two counties, OC has the superior surf and sand. When people think of California's bright and sunny beaches, they're envisioning Surf City, USA and the Wedge -- not Redondo. Heal the Bay's annual Beach Report Card named three Los Angeles beaches in their Top 10 Beach Bummers list of the most polluted California beaches of 2015. Orange County had only one: Huntington State Beach came in at 10th. Huzzah for almost not being on a bad list!!!
Trader Joe's vs. Ralphs: A Definitive Infographic of Which Is the Better Deal
Flickr/World Bank Photo Collection
Orange County actually breeds Los Angeles' talents
LA gets the credit, but you can thank OC for breeding the likes for Gwen Stefani, Tiger Woods, Roy Choi, Will Ferrell, and countless more talents from all walks of life. Don't like any of them? Undeniable talents like Marlon Brando, Dita von Teese, and Steve Martin all cut their teeth here, too. And of course, once the stars are done with the pretension and BS of Tinseltown, they inevitably come south to get away from it all. Looking at you, Kobe, John Wayne, Philip K Dick and, uh, Jenna Jameson?
Flickr/John Watson
This one's a duh, but Anaheim is home to, modestly, THE GREATEST THEME PARK OF ALL TIME. People travel from all over the world just to come to Disneyland. People travel up to 25 minutes if the traffic's not that bad to come to Universal Studios. The recent and pending addition of the Simpsons and Harry Potter expansions might draw in nerds from around the globe but the Mouse House has had a steady following from Disnerds since the 50's. And when Disney's Star Wars Land expansion opens? Game over.
Orange County smells better
You'll typically only smell human urine on the streets of Orange County after a wild weekend night in our county's few downtowns. A day in Los Angeles is a day spent playing, "What's That Offensive Odor?" and nobody wins. A look at the American Lung Association's State of the Air 2015 report reveals that, yeah, we both failed in two of the three main air pollution categories: Ozone and Particle Pollution 24-hour. But guess what? OC did pass in the Particle Pollution Annual category and LA failed by a significantly larger margin. So you guys suck more, comparatively! Also, OC asks, giant apocalyptic gas leak who?
Flickr/Paul Narvaez
We're stealing your music scene
Once upon a time, popular music acts would stop in LA and then pass right on through OC on their way to San Diego, stopping here probably only to pee unless they'd already done that on the streets of LA. The last half-a-decade has changed all of that (minus the peeing), thanks to the likes of Burger Records and the Observatory concert venue. Now big acts will skip LA to come play at the Observatory or Constellation Room, and festivals like the Growlers' annual Beach Goth and the crazy-diverse Burgerama bring tons of bands -- and fans -- up from LA. And speaking of Burger Records, it's the buzziest label in SoCal… and it operates out of a little lime green room in a Fullerton industrial park.
Flickr/Jennifer
Our food scene is a force to be reckoned with
Orange County has cultivated world class chefs for decades. The problem was, they almost always felt the need to move on to bigger cities to make a name for their talent and to experiment. Not so anymore. Orange County is now a destination for celebrity chefs—homegrown or imported—to start their food empire. Roy Choi of the Kogi truck fame is an Orange boy and his parents owned a restaurant in Anaheim. We have Jason Quinn who took on the Food Network with the Lime Truck and won before taking on the status quo of the restaurant industry with his Playground restaurant in Santa Ana. We have Amar Santana building his dining empire with Broadway and now Vaca. And if young, hip chefs aren't your thing -- we were the county to bring back Southern California fast food cult favorite Naugles in 2015, 25 years after it folded.
Orange County has less traffic
While driving on the 405 N between the 55 and Long Beach at 5pm is something you'd only wish on a bad ex or evil boss or both, driving in the vast majority of Los Angeles -- freeway or street -- is a punishment that should be reserved for tow truck drivers and puppy killers.
So the Los Angeles Times reported in late 2015 by way of the American Highway Users Alliance, that Seal Beach has the distinct honor of the number two worst traffic bottleneck in Southern California. 10 more stretches of freeway from Los Angeles County are in the top 30. And when you look at OC's only mention on the list, you realize it blocks up... right at the Los Angeles County Line.
When Foodie Met Truckie: The Story of Food Trucks in LA
Flickr/Richard Daugherty
It's less crowded in Orange County
"It's more crowded in Los Angeles because more people want to be here," you may quip. Wrong. No one wants to be anywhere where it takes 45 minutes to park and walk to your destination, just to wait in an hour line to get into an oversold event, over-paying all the way down the line for the privilege. The US Census Bureau says Los Angeles County had 10.11 million people call it home in 2014, while Orange County had 3.01 million folks. You may say LA's more popular for a reason, but we say that's 7.1 million less assholes peeing all over everything.
Oh yeah: free parking everywhere
Because paying $5-$30 every time you go out is for chumps.
Sign up here for our daily LA email and be the first to get all the food/drink/fun Los Angeles has to offer.
Taylor Hamby is the Web Editor at OCWeekly.com. When she's not telling the stories of the freaks and geeks of Orange County, she can be found drinking in a costume, partying like it's 1899. You can find her at @TaylorWrites on Twitter.


text:
Léon Jean, né le  à Lunel-Viel (Hérault) et mort le  à Montpellier (Hérault), est un mutualiste et homme politique français.

Biographie
Ouvrier agricole, puis exploitant agricole, viticulteur, Léon Jean milite au sein du syndicat CGT local, dont il devient le secrétaire en 1930.  Il s'investit aussi dans le militantisme mutualiste, et assure, à partir de 1929, la présidence de la société mutualiste L'Avenir, puis, de 1939 à 1946, celle de la caisse départementale des assurances sociales.

Membre du parti socialiste SFIO depuis 1920, il se présente en 1929 aux municipales, sur une liste d'union socialiste et radicale, qui est battue. En 1932, de nouveau candidat lors d'élections complémentaires, il est élu et devient le premier adjoint d'Antoine Jullian, au sein d'une municipalité socialiste et républicaine-socialiste.

En 1937,  il est élu conseiller d'arrondissement, dans le canton de Lunel.

Sans activité de résistance pendant la guerre, il démissionne néanmoins dès 1940 de son mandat municipal.

Après la seconde guerre mondiale, il est élu conseiller général de l'Hérault, dans le canton de Lunel, en 1945, puis maire de Lunel-Viel en 1947, et sera constamment réélu par la suite.

Il reprend aussi ses activités mutualiste : membre du conseil supérieur des assurances sociales en 1945, il est président de la caisse primaire d'assurance maladie de l'Hérault de 1953 à 1967.

En 1951, il est placé en troisième position sur la liste socialiste, menée dans l'Hérault par Jules Moch, aux élections législatives. Grâce à un large apparentement des listes de la « troisième force », la SFIO obtient trois sièges, et Léon Jean est élu député.

Comme plusieurs autres parlementaires héraultais, il s'intéresse principalement à l'Assemblée aux questions viticoles, centrales dans la vie économique de son département. Il défend notamment la création d'aides de l'Etat pour les exploitants victimes d'intempéries ou faisant face à des difficultés financières. Il dépose aussi, en 1955, un rapport visant à créer un comité interprofessionnel des vins des Côtes de Provence.

Cela ne l'empêche pas de participer aussi aux débats sur la question des retraites, en 1952 et 1954, défendant des positions conformes aux mandats de son parti, et fort de son expertise mutualiste.

En 1956, il n'est pas réélu député, et tente vainement, deux ans plus tard, de retrouver l'Assemblée nationale. Il se consacre ensuite à ses mandats locaux, jusque dans les années 1970 : conseiller général jusqu'en 1973, et maire jusqu'en 1977.

Il poursuit aussi son engagement mutualiste, comme président de l'union départementale de la mutualité de 1963  à 1983.

Sources
Biographie sur le site de l'Assemblée nationale

Dictionnaire biographique du mouvement ouvrier français, notice d'Olivier Dedieu et Jean Sagnes

Député de l'Hérault
Section française de l'Internationale ouvrière
Mutualité
Naissance en janvier 1901
Décès en décembre 1986
Décès à Montpellier
Décès à 85 ans
Naissance dans l'Hérault

redpajama_set_name: RedPajamaWikipedia


Windows Phone is the latest mobile phone operating system from Microsoft. It has caught the attention of developers. This is due to the fact that the learning curve to start Windows Phone developments is minimal for those who are already familiar with .NET developments. People who master the developments of applications for Windows Phone stand to gain a lot with demands for such developers picking up. A half-a-day event is planned at Mysore to give an introduction to the programming for Windows Phone. This event will highlight the Windows Phone developments using .NET. There are some ongoing competitions for developers and students. Developers have to develop, submit and get approved 3 applications on the Windows Phone market place. Similar scheme is available for students with the difference that they have to submit 4 apps. This will be a great opportunity for the developers and students to get an introduction to Windows Phone developments. Not only they can learn the Windows Phone developments, they can also get a brand new Windows Phone if they fulfill the conditions. The details will be announced during the event.
Dr U B Pavanaja holds Master's degree from Mysore University and PhD from Mumbai University. He was a scientist at Bhabha Atomic Research Centre, Mumbai, for about 15 years. He has done advanced research at Taiwan. He resigned BARC in 1997 and dedicated himself fully for the cause of Computer and Indian languages. He has to his credit many firsts, viz., first Kannada web-site, first Kannada online magazine, first Indian language (Kannada) web-site to receive Golden Web Award, first Indian language (Kannada) editor for Palm OS, first Indian language (Kannada) editor for WinCE device (HP Jornado 720), first Indian language version (Kannada) of universally popular Logo (programming language for children) software, etc. his Kannada Logo has won the Manthan Award for the year 2006. He was a member of the Technical Advisory Committee setup by Govt of Karnataka on Standardization of Kannada on Computers (2000). He is also the member of Kannada Software Committee of Govt of Karnataka (2008-current). He started his career on computers from FORTRAN and then moved on to Pascal, C, BASIC, QuickBasic, Visual Basic, VB.Net, etc. He has attended and represented Indian languages in many Indian and International forums like Indic Font Workshop (Indic Computing Consortium, Bangalore, India), Unicode conference (Unicode Consortium, CA, USA), OpenType Font Seminar (Microsoft, Seattle, USA), etc. He is quite well known in Indic computing arena. He is also popular as a writer of articles in Kannada about IT. He has consulted to Microsoft India and Microsoft Research Labs India. His last job was at Excelsoft Technologies, Mysore as Evangelist & Mentor. Currently he is heading his own venture called Vishva Kannada Softech.
Goutham Upadhyaya works as a Partner Technical Consultant at Microsoft from two years. Having around 5+ years of IT experience and worked with Satyam and Wipro before joining Microsoft. His role involves guiding partners in adopting and implementing latest Microsoft technologies. He is passionate about Microsoft technologies and worked on NET 4.0, Silverlight, WPF,Windows Mobile/Phone7 and Asp.Net. Also, works on emerging technologies like Webmatrix ,RIA Services, Windows Azure, Visual Studio LightSwitch, Entity Framework and LINQ. On a personal front he likes traveling and spending time with friends and Family.


text:
Ani DiFranco and Utah Phillips - The Past Didn't Go Anywhere
Name -
CD / - - $15.00
Decrease quantity for Ani DiFranco and Utah Phillips - The Past Didn't Go Anywhere
Increase quantity for Ani DiFranco and Utah Phillips - The Past Didn't Go Anywhere
U. Utah Phillips was a 61-year-old traveling storyteller, songwriter, and political activist whose contributions to folk music are legendary. Ani DiFranco was a 26-year-old singer-songwriter whose recordings and live shows had earned her a devoted following among alternative rockers and hard-core folkies alike. They came together on The Past Didn't Go Anywhere, the first album by an outside artist released on DiFranco's Righteous Babe label.
The collaboration started with Utah sending Ani two decades of master tapes of his live performances. Ani was captivated by the stories Utah used to introduce his songs, so she decided to take the unexpected route and put them in the spotlight. She hand selected a wide variety of his tales and set them to surprising but beautifully fitting music. The result is a unique juxtaposition of storyteller and musician.
At the core of the project are the rhythms of Utah's twisting, intertwined narratives. Among his cast of real-life characters are hobos, hustlers, politicians, and other scoundrels whose adventures form a cross-country, cross-generational journey through the bars, supermarkets, campuses, and ghost towns of America. Tying the whole thing together are Ani's instrumental settings, layering train whistles, found soundbites, classical piano, slide guitar, and drum samples while incorporating elements of funk, country, and rap music to create a musical journey through Utah's life.


Health reasons. Due to removal of gallbladder my husband was not able to eat yeasted bread, and I had started to search for other options and solutions to leaven my bread.
I normaly keep my starter int the fridge, as I don't bake that often, 2-3 times a week. When I feed my starter, I sometimes do multiple feedings in one day, in the morning, then after 4 hours I feed it again, during that time I leave it on the kitchen counter. Then I usually make 60% motherdough/sometimes I use liquid levain.
When I first made my sourdough I made it with stoneground rye and filtered water. Then after a year and a half I started feeding it with semi-white stone ground wheat, and after 2 years I lowered the hydration from 100% to 80%.
You can use it for all kinds of bread dough and sweet dough.


text:
Edde or EDDE can refer to:

 Edde, Hungary, a village in Somogy county, Hungary
 Edde, Lebanon, a village located 45 km north of Beirut, Lebanon
 The ICAO airport code for Erfurt–Weimar Airport in Erfurt, Germany

See also
 Edde (surname)


On June 30, 2016 at approximately 1:00 a.m., Animal Control responded to assist Anne Arundel County Police with an injured cat found inside a home at the 8300 block of Hope Point Court. Anne Arundel County Police Officers had concerns for the animal's well-being and immediately contacted Animal Control to assist with providing veterinary treatment for the cat. The cat, dubbed Charlie, was transported to the Anne Arundel County Emergency Veterinary Hospital where he was stabilized overnight. Later in the morning Charlie was picked up from AAVEC and transported to Waugh Chapel Animal Hospital by Animal Control for long term treatment.
According to veterinary documents Charlie sustained burns over a large portion of his body approximately ten days to two weeks prior to Charlie being found by AACOPD. Charges of animal cruelty have been filed against the owner of the cat, Sean Todd McDermott, 53, of Hope Point Court in Millersville.
Charlie is expected to fully recover but he will have a long road ahead and need extensive treatments due to the nature of his wounds. Anne Arundel County Animal Control is grateful to Waugh Chapel Animal Hospital who maintains an account for use for our animals that need more treatment than the shelter can provide. Monetary donations are accepted to this account from individuals wishing to help with Charlie's recovery or donations could be made to Friends of Anne Arundel County Animal Control for "Charlie". Charlie is not currently available for adoption but Anne Arundel County and Waugh Chapel have hopes for a full recovery and for him to be adopted in to a loving new home.


text:
Tech meets fish: Port of New Bedford launches 'Ocean Cluster'
City of New Bedford, Innovation, News, Port of New Bedford
By Jennette Barnes
Updated Sep 21, 2017 at 6:32 PM
If every part of a fish were used for high-value products, the New Bedford fishing industry could make more money from fewer fish.
That kind of innovation is what's behind a new effort by New Bedford Harbor Development Commission to serve as a matchmaker for technology companies and the fishing industry. Following a model developed in Iceland, the commission has formed the New Bedford Ocean Cluster, which will foster entrepreneurship in ocean products.
Mayor Jon Mitchell, who chairs the commission, signed a memorandum of understanding Thursday with Thor Sigfusson, founder and chairman of the Iceland Ocean Cluster, to work together. The agreement officially makes New Bedford part of a loosely organized global network of ocean clusters. No money will change hands; it's about an exchange of ideas, Sigfusson said.
New Bedford's is the third such effort worldwide, following Iceland and Maine. Others are forming in Alaska and Seattle.
Mitchell said New Bedford wants to be associated with all things fishing — not just fish and fish processing, but pharmaceuticals, cosmetics, and other products.
"This is really, for us in New Bedford, a way of taking the next step," he told supporters gathered at the New Bedford Whaling Museum for a signing ceremony. "Networks matter. Idea exchanges matter. And that's what this is about."
The Iceland Ocean Cluster operates a business incubator with more than 60 businesses.
"We want to be a spin-off factory," Sigfusson said.
From 1981 to 2011, Iceland doubled its cod export revenue to $680 million, even though the catch fell 60 percent, he said. It accomplished that by diversifying the products made from cod.
In 1981, 75 percent of Iceland's cod revenue came from fillets and whole fish, and 25 percent from other products, he said. By 2011, the market had reversed, with 77 percent of revenue coming from other products — things like dietary supplements and fish-skin leather.
New Bedford-based technology company IoT ImpactLABS is working with the Harbor Development Commission on the project, organized by the commission's executive director and port director, Edward Anthes-Washburn. The port has piloted new technologies through its own facilities and by connecting ImpactLABS entrepreneurs with existing port users and businesses, Anthes-Washburn said.
In an interview after the signing, Sigfusson said he was impressed with the new UMass Dartmouth School for Marine Science and Technology facility. It would be a great place to host startups and have students working on ocean-related entrepreneurial projects, he said.
Follow Jennette Barnes on Twitter @jbarnesnews.
Original here:


User Name* Is this User Name available?
The password should be 10 to 15 characters long.
Security Question 1* Select Security Question Wedding anniversary? Father's middle name? Favorite movie? Favorite sports team? Favorite teacher's name? First child's middle name? High school name? Mother's maiden name? Spouse's middle name? What is the color of your first car? Date of birth? What is your GIN Number?
Security Question 2* Select Security Question Wedding anniversary? Father's middle name? Favorite movie? Favorite sports team? Favorite teacher's name? First child's middle name? High school name? Mother's maiden name? Spouse's middle name? What is the color of your first car? Date of birth? What is your GIN Number?


Luke Thompson is a part of the Permanent Projects and Programmes team at La Fosse Associates, specialising in Recruiting for Business Analyst.
Prior to joining La Fosse, Luke attended The Peter Jones Enterprise Academy where he studied business enterprise. Following university, he worked in the fitness industry as a membership sales consultant for 3 years.


text:
// Copyright 2015 The Chromium Authors. All rights reserved.
// Use of this source code is governed by a BSD-style license that can be
// found in the LICENSE file.

/**
 * @fileoverview 'settings-startup-urls-page' is the settings page
 * containing the urls that will be opened when chrome is started.
 */

import 'chrome://resources/js/action_link.js';
import 'chrome://resources/cr_elements/action_link_css.m.js';
import 'chrome://resources/polymer/v3_0/iron-flex-layout/iron-flex-layout-classes.js';
import 'chrome://resources/polymer/v3_0/iron-list/iron-list.js';
import '../controls/extension_controlled_indicator.js';
import '../settings_shared_css.js';
import './startup_url_dialog.js';

import {CrScrollableBehavior} from 'chrome://resources/cr_elements/cr_scrollable_behavior.m.js';
import {assert} from 'chrome://resources/js/assert.m.js';
import {focusWithoutInk} from 'chrome://resources/js/cr/ui/focus_without_ink.m.js';
import {WebUIListenerMixin, WebUIListenerMixinInterface} from 'chrome://resources/js/web_ui_listener_mixin.js';
import {mixinBehaviors, PolymerElement} from 'chrome://resources/polymer/v3_0/polymer/polymer_bundled.min.js';

import {EDIT_STARTUP_URL_EVENT} from './startup_url_entry.js';
import {getTemplate} from './startup_urls_page.html.js';
import {StartupPageInfo, StartupUrlsPageBrowserProxy, StartupUrlsPageBrowserProxyImpl} from './startup_urls_page_browser_proxy.js';

const SettingsStartupUrlsPageElementBase =
    mixinBehaviors(
        [CrScrollableBehavior], WebUIListenerMixin(PolymerElement)) as {
      new ():
          PolymerElement & WebUIListenerMixinInterface & CrScrollableBehavior
    };

export class SettingsStartupUrlsPageElement extends
    SettingsStartupUrlsPageElementBase {
  static get is() {
    return 'settings-startup-urls-page';
  }

  static get template() {
    return getTemplate();
  }

  static get properties() {
    return {
      prefs: Object,

      /**
       * Pages to load upon browser startup.
       */
      startupPages_: Array,

      showStartupUrlDialog_: Boolean,
      startupUrlDialogModel_: Object,
      lastFocused_: Object,
      listBlurred_: Boolean,
    };
  }

  prefs: Object;
  private startupPages_: Array<StartupPageInfo>;
  private showStartupUrlDialog_: boolean;
  private startupUrlDialogModel_: StartupPageInfo|null;
  private lastFocused_: HTMLElement;
  private listBlurred_: boolean;
  private browserProxy_: StartupUrlsPageBrowserProxy =
      StartupUrlsPageBrowserProxyImpl.getInstance();
  private startupUrlDialogAnchor_: HTMLElement|null;

  constructor() {
    super();

    /**
     * The element to return focus to, when the startup-url-dialog is closed.
     */
    this.startupUrlDialogAnchor_ = null;
  }

  override connectedCallback() {
    super.connectedCallback();

    this.addWebUIListener(
        'update-startup-pages', (startupPages: Array<StartupPageInfo>) => {
          // If an "edit" URL dialog was open, close it, because the underlying
          // page might have just been removed (and model indices have changed
          // anyway).
          if (this.startupUrlDialogModel_) {
            this.destroyUrlDialog_();
          }
          this.startupPages_ = startupPages;
          this.updateScrollableContents();
        });
    this.browserProxy_.loadStartupPages();

    this.addEventListener(EDIT_STARTUP_URL_EVENT, (event: Event) => {
      const e =
          event as CustomEvent<{model: StartupPageInfo, anchor: HTMLElement}>;
      this.startupUrlDialogModel_ = e.detail.model;
      this.startupUrlDialogAnchor_ = e.detail.anchor;
      this.showStartupUrlDialog_ = true;
      e.stopPropagation();
    });
  }

  private onAddPageTap_(e: Event) {
    e.preventDefault();
    this.showStartupUrlDialog_ = true;
    this.startupUrlDialogAnchor_ =
        this.shadowRoot!.querySelector('#addPage a[is=action-link]');
  }

  private destroyUrlDialog_() {
    this.showStartupUrlDialog_ = false;
    this.startupUrlDialogModel_ = null;
    if (this.startupUrlDialogAnchor_) {
      focusWithoutInk(assert(this.startupUrlDialogAnchor_));
      this.startupUrlDialogAnchor_ = null;
    }
  }

  private onUseCurrentPagesTap_() {
    this.browserProxy_.useCurrentPages();
  }

  /**
   * @return Whether "Add new page" and "Use current pages" are allowed.
   */
  private shouldAllowUrlsEdit_(): boolean {
    return this.get('prefs.session.startup_urls.enforcement') !==
        chrome.settingsPrivate.Enforcement.ENFORCED;
  }
}

declare global {
  interface HTMLElementTagNameMap {
    'settings-startup-urls-page': SettingsStartupUrlsPageElement;
  }
}

customElements.define(
    SettingsStartupUrlsPageElement.is, SettingsStartupUrlsPageElement);

redpajama_set_name: RedPajamaGithub


In the first part I talked about using the Content-Type and Accept HTTP headers to allow a single website to be use both by humans and programs.
In the previous part I gave a decorator which can be used to make working with JSON very easy. For our use though this isn't great because a view decorated in this way only accepts JSON as the POST body and only returns JSON, regardless of the HTTP headers.
The decorator given below relies on a django snippet to decode the Accept header for us so don't forget to added it to your middleware.
So, how can we use this decorator? Let's imagine we're creating a blog and we have a view which displays a post on that blog. If they user posts it should create a new comment. Firstly we create a function, common, which gets the blog object and returns a 404 if it doesn't exist. The return of this function is passed onto all other functions as their arguments.
Next we write two functions to handle the cases where the users POSTs a form encoded body, or some JSON. The return values of these functions are passed onto the chosen output function as the arguments.
The JSON output function doesn't need to return an HttpResponse object like a normal Django view because the output is automatically encoded as a string and wrapped in a response object.
Finally we come to the HTML output function. This function is also called if not mime type in Accept is suitable.
This decorator is really little more than a sketch. Many more content types could be supported, but hopefully it gives a good example of how you can write a very flexible webservice and still reduce code duplication as much as possible.
Building a RESTful webservice is pretty straight-forward with Django, but in many cases you want to have both a human readable website and a machine readable api. A lot of websites solve this problem by using http://www.x.com as the human site, an api.x.com as the machine site. They also will typically have different structures to support the different usecases.
Unless your documentation is really excellent and the person writing the client to your service actually reads it building a client for the service is an error prone process. In an ideal world the developer would be able to browse the website and use the same urls in their client program. Fortunately HTTP has two headers which make it possible to do just that, Content-Type and Accept.
The Content-Type header describes the type of data that is included in the body of the HTTP request. Typically this will be values such as text/html, application/json or application/x-www-form-urlencoded. A content type is sent by the client when POSTing or PUTing data, and whenever the webserver includes some data in its response. The Accept header is sent by a client to specify what content types it can accept in the response. This header has a more complicated format that Content-Type because it can used to specify a number of different content types and to give a weighting to each.
When combined these two headers can be used to allow a normal user to browse the site and to allow a robot to make api calls on the same site, using the same urls. This makes it easier both for the creator of the programmer accessing your site and for you because you can easily share code between the site and your api.
I'm going to outline a decorator that will let write a webservice such as this, that will support HTML and JSON output, and JSON and form encoded data as inputs.
First we'll create a decorator that parses any post data as JSON and passes it the view as the second parameter (after the request object). It will also JSON encode any return value that's not an HTTPResponse object.
This decorator should be pretty easy follow, but here is an example to illustrate its use.
This really cuts down on the code you need to write, but this view only handles JSON as its input and output. Next we need to parse the Accept headers and return an ordered list of content types so we can choose the preferred option. No need to reinvent the wheel, so we just pull some code from djangosnippets.org.
All the parts are in place now, and in my next post we'll create a decorator which takes these parts ands puts them together.