text:
\section{Introduction}
The redshifted 21-cm emission from the discrete, unresolved neutral
hydrogen (HI) sources in the post-reionization era ($z < 6$) appears
as a faint diffuse background radiation in low frequency observations
below 1420 MHz. This provides us a useful tool to explore the large
scale structure of the universe in the post-reionization era, using
the fluctuations in the diffuse background radiation to trace the HI
power spectrum (Bharadwaj, Nath \& Sethi 2001; Bharadwaj \& Sethi
2001). In addition to probing the HI power spectrum (Bharadwaj \&
Pandey 2003; Bharadwaj \& Srikant 2004), fluctuations in the diffuse
background radiation also probe of the bispectrum (Ali et al. 2006;
Guha Sarkar \& Hazra 2013). In recent years, a considerable amount of
work has been done to explore the prospects of detecting the 21-cm HI
signal from the post-reionization era (Visbal et al. 2009; Bharadwaj
et al. 2009; Wyithe \& Loeb 2009; Seo et al. 2010; Mao 2012; Ansari et
al. 2012; Bull et al. 2014).

 In the post-reionization era, the bulk of the HI 21-cm emission
 originates from the dense pockets of self-shielded HI regions, which
 are identified as damped Ly$\alpha$ (DLA) systems in quasar
 observations.  The fluctuations in the HI 21-cm emission which are in
 general quantified through HI power spectrum, is expected to trace
 the matter power spectrum with a possible bias (Bharadwaj, Nath \&
 Sethi 2001; Bharadwaj \& Sethi 2001). Wyithe \& Loeb (2009) have
 shown that the complications in the HI power spectrum arising due to
 the modulation of the ionizing field are less than 1\%. Bagla,
 Khandai \& Datta (2010) have used semi-numerical simulations to
 predict the HI bias. They have used three different prescriptions to
 assign HI mass to the dark matter haloes and have found the HI bias
 to be scale-independent on large scales ($k \leq 1$ Mpc$^{-1}$). Guha
 Sarkar et al. (2012) and Vilaescusa Navarro et al. (2014) have used
 simillar simulations and their results are also found to be
 consistent with a scale-independent HI bias on large
 scales. Recently, Sarkar, Bharadwaj \& Anathpindika 2016 have used
 semi-numerical simulations to model the HI bias and have provided a
 fitting formula for the HI bias $b_{HI}(k,z)$ in both $k$ and $z$
 across $0.01 \leq k \leq 10$ Mpc$^{-1}$ and $0 \leq z \leq 6$.

The measurement of the HI power spectrum holds the possibility of
constraining the background cosmological model through the Baryon
Acoustic Oscillations (BAO) (Wyithe et al. 2008; Chang et
al. 2008). Seo et al. (2010) have studied the possibility of measuring
BAO using the HI power spectrum with a ground-based radio
telescope. The measurement of the HI power
spectrum can also be used to constrain cosmological parameters
independent of the BAO (Bharadwaj et al. 2009; Visbal, Loeb \& Wyithe
2009). The measurement of the HI power spectrum can also be used to
constrain the neutrino mass (Loeb \& Wyithe 2008). Villaescusa Navarro
et al. (2015) have used hydrodynamical simulations to study the
signatures of massive neutrinos on the HI power spectrum and put
constraints on the neutrino mass. In a recent work, Pal \& Guha Sarkar
(2016) have studied the prospects of measuring the neutrino mass using
the HI 21-cm and the Ly-$\alpha$ forest cross-correlation power
spectrum.

Measurements of the HI power spectrum are sensitive to both the mean
neutral hydrogen fraction $\Omega_{HI}(z)$ and the HI bias
$b_{HI}$. Several measurements have been carried out in past years to
measure the value of the $\Omega_{HI}$ both at low and at high
redshifts. Measurements of the $\Omega_{HI}$ at low redshifts ($z \leq
1$) come from HI galaxy surveys (Zwaan et al. 2005; Martin et
al. 2010; Delhaize et al. 2013), DLAs observations (Rao et al. 2006;
Meiring at al. 2011) and HI stacking (Lah et al. 2007; Rhee at
al. 2013), while measurements of $\Omega_{HI}$ at high redshifts ($1 <
z < 6$) are from DLAs studies (Prochaska \& Wolfe 2009; Norterdaeme et
al. 2012; Zafar et al. 2013). Measurement of the HI power spectrum can
provide astrophysical information about the HI distribution.

Efforts have been made to measure the $\Omega_{HI}$ at redshifts $z <
1$. Chang et al. (2010) and Masui et al. (2013) have studied the
cross-correlation of the HI intensity and the galaxy surveys, while
Switzer et al. (2013) have studied the autocorrelation of HI intensity
to measure the $\Omega_{HI}$. Ghosh et al. (2012) have used the GMRT
observations to place a upper limit on the value of $\Omega_{HI}$ at
$z = 1.33$.

Several low frequency radio interferrometric arrays
(CHIME\footnote{http://chime.phas.ubc.ca/}, Bandura et al. 2014;
BAOBAB\footnote{http://bao.berkeley.edu/}, Pober et al. 2013) are
planned to measure the BAO using the 21-cm signal from $z \leq
2.55$. Shaw et al. (2014) present theoretical estimates for the
sensitivity of CHIME to constrain the line-of-sight and angular scale
of the BAO.  The Giant Meterwave Radio Telescope (GMRT
\footnote{http://gmrt.ncra.tifr.res.in/}, Swarup et al. 1991)
which operates at frequencies corresponding to HI in the redshift
range $0 \leq z \leq 8.5$. The GMRT is currently being upgraded. The
prospects of detecting the HI power spectrum from the post
reionization era for the upgraded GMRT (uGMRT) has been studied in
Chatterjee et al. (2016). The proposed future telescopes SKA1-mid and
SKA1-low \footnote{https://www.skatelescope.org/home/technicaldatainfo/key-documents/},
both hold the prospect of measuring the post-reionization HI power
spectrum at a high level of precision (Guha Sarkar \& Datta 2015; Bull
et al. 2015; Santos et al. 2015).

There is a rich literature on the sensistivity estimates for various
low frequency radio telescopes. Morales et al. (2005) present a
general method to calculate the Epoch of Reionization (EOR) power
spectrum sensitivity for any radio-interferrometric array. Harkar et
al. (2010) have made sensitivity estimates for the Low Frequency Array
(LOFAR{\footnote{http://www.lofar.org/}}, van Haarlem et
al. 2013). Simillar estimates have been made in the context of the
Murchison Wide-field Array
(MWA{\footnote{http://www.mwatelescope.org}}, Bowman et al. 2013;
Tingay et al. 2013). Beardsley et al. (2013) have estimated the
sensitivity of the MWA to the EOR 21-cm power spectrum and McQuinn et
al. (2006) present estimates for cosmological parameter estimation
using MWA5000, a hypothetical extended version of MWA.  Parsons et
al. (2012) have explored redundancy calibration in the context of the
Donald C. Backer Precision Array to Probe the Epoch of Reionization
(PAPER{\footnote{http://astro.berkeley.edu/dbacker/eor}}, Parsons et
al. 2010).  Pober et al. (2014) have studied the constraints
acheiveable with the Hydrogen Epoch of Reionization Array
(HERA{\footnote{http://reionization.org/}}, DeBoer et al. 2016; Neben
et al. 2016) and have found that a very high significance ($~\rlap{$>$}{\lower 1.0ex\hbox{$\sim$}} \,
30\sigma$) detection of the reionization power spectrum is possible in
even the most pessimistic scenarios.  Aaron Ewall-Wice et al. (2016)
have used the Fisher matrix formalism to predict the sensitivity with
which it will be possible to constrain reionization and X-ray heating
models with the future HERA and SKA phase I.

Here, we discuss the prospects of measuring the HI power spectrum at
$z \sim 3$, using the upgraded Ooty radio Telescope (ORT). The ORT
consists of a 530 m long and 30 m wide parabolic cyllindrical
reflector, which is placed in the north-south direction on a hill
having the same slope as the latitude (11$^{o}$) of the station
(Swarup et al. 1971; Sarma et al. 1975). It is possible to observe the
same part of the sky through a single rotation of the long axis, which
is aligned with earth's rotation axis. The entire feed system of the
ORT has 1056 dipoles, spaced 0.47 m apart from each other, which are
placed along the focal line of the telescope. The cyllindrical Ooty
Radio Telescope (ORT) is currently being upgraded (Prasad \&
Subrahmanya 2011a, b; Marthi \& Chengalur 2014, Subrahmanya 2017a, b) to function as a
linear radio interferrometric array the Ooty Wide Field Array
(OWFA). The OWFA works at a nominal frequency of $\nu_{0} = 326.5$
MHz, which corresponds to HI radiation from the redshift $z =
3.35$. The OWFA can operate in two independenet interferrometric modes
- Phase I and Phase II. In this work, we have considered Phase II
only. The Phase II has 264 antenna elements, where each antenna
element consists of 4 dipoles. Each antenna has a rectangular aperture
of dimension 1.92 m $\times$ 30 m. The field-of-view of OWFA Phase II is highly
assymetric in dimension, $27.4^{o} \times 1.75^{o}$. The operating
bandwidth for the Phase II is 40 MHz. The field-of-view and the
observing bandwidth of the OWFA Phase II allow to observe the universe over a
real space volume $\sim 0.3 \, {\rm Gpc}^3$.

We now report some recent works related to OWFA. Calibration is an
important issue for OWFA and it has been addressed in Marthi \&
Chengalur (2014). Gehlot \& Bagla (2017) have followed the approach of
Ali \& Bharadwaj (2014) to predict the HI signal expected at
OWFA. Marthi (2017) presents a programmable emulator for simulating
OWFA observations for which foreground modelling and predictions are
presented in Marthi et al. (2017). Chatterjee, Bharadwaj \& Marthi
(2017) present simulations of the HI signal expected at OWFA.

Ali \& Bharadwaj (2014) (hereafter, Paper I) have studied the prospects of detecting the
21-cm signal using OWFA. In this paper, We have also made detailed
foreground predictions for OWFA. In a recent study, Bharadwaj, Sarkar
\& Ali (2015)(hereafter, Paper II) have used the Fisher matrix analysis to make predictions
for hours of observations to measure the HI power spectrum. We showed
that the dominant contribution to the OWFA HI signal is from the
$k$-range $0.02 \leq k \leq 0.2$ Mpc$^{-1}$. It was found that a
$5\sigma$ detection of the HI power spectrum is possible with $\sim
150$ hours of observations using the Phase II. In this study, we have also
explored the possibility of measuring the redshift space distortion
parameter $\beta$. We found that the non-uniform sampling of the
$\mathbf{k}$-modes does not make OWFA suitable for measuring $\beta$.

The predictions for OWFA, mentioned earlier, have all assumed that the
HI power spectrum is related to the $\Lambda$CDM power spectrum with a
scale-independent linear HI bias. All of these studies have focussed
on measuring the amplitude of the HI power spectrum assuming that the
shape of the matter power spectrum (Eisenstein \& Hu 1998) is
precisely known. It is interesting and worthwhile to consider a
situation where both amplitude and the shape of the HI power spectrum
is unknown. There are several astrophysical processes which could in
principle, change the shape of the HI power spectrum without affecting
the matter power spectrum. Further, uncertainties in the background
cosmological model would also be reflected as changes in the observed
HI power spectrum through various effects like redshift space
distortion and Alcock-Paczynski (AP) effect. In this paper, we have
considered the possibility of measuring the HI power spectrum using
OWFA. For this purpose, we have divided the $k$-range into several
bins and employed the Fisher matrix analysis to make predictions for
measuring the HI power spectrum in each of these $k$-bins. Throughout
our analysis, we have used the $\Lambda {\rm CDM}$ cosmology with
PLANCK+WMAP9 best-fit cosmological parameters (Ade at al. 2014).

The paper is structured as follows. In section 2, we present the
theoretical HI model which was used for calculating the signal and
noise covariance. Here we also show the Fisher matrix technique which
was employed for estimating the binned HI power spectrum. In section
3, we use the results from the Fisher matrix analysis to make
predictions for measuring the binned 21-cm power spectrum. We end with
summary and conclusions in Section 4.

\section{Visibility covariance \& Fisher matrix}

OWFA measures visibilities $\mathcal{V}(\mathbf{U}_a, \nu_n)$ at given
baselines $\mathbf{U}_a$ and frequency channel $\nu_{n}$. The baseline
configuration of the OWFA is one-dimensional. It consists of 264
antennas, arranged in a linear array along the length of the
cylinder. Assuming the $\mathbf{x}$-axis to be along the length of the
cylinder, the baselines of the OWFA can be written as follows, i.e,
\begin{equation}
\mathbf{U}_{a} = a \left(\frac{d}{\lambda}
\right)\hat{i} \hspace{2.5cm} (1 \leq a \leq 263)
\end{equation}
where $a$ denotes the baseline number, $d=1.92$ m, is the distance
between two consecutive antennas and $\lambda$ is the wavelength
corresponding to the central observing frequency $\nu_0$. OWFA has a
high degree of redundancy in baselines. For OWFA, any given baseline
$\mathbf{U}_{a}$ occurs $(264-a)$ times in the array. This can be used
to both calibrate the antenna gains (independent of the sky model) as
well as to estimate the true visibilities (marthi \& Chengalur 2014).

In reality baselines $\mathbf{U}_{a}$ change as frequency
  varies across the observing bandwidth $(B)$. This is an extremely
  important factor that needs to be taken into account in the actual
  data analysis. The expected fractional variation in the baseline
  $\Delta U/U$, about the central frequency $\nu_0$ over the bandwidth
  of observation is $\Delta U / U = B/2\nu_0 \sim 4.5\%$ for $B =30$
  MHz. This is not significant enough to consider in our analysis and
  we have kept the baselines fixed at the value, corresponding to the
  central frequency $\nu_0$. The actual bandwidth may be somewhat
  larger than $B =30$ MHz.

We express the telescope's observing frequency bandwidth as $B = N_c
\Delta \nu_c$ where $N_c$ is the number of the frequency channels and
$\Delta \nu_c$ is the channel-width. For our analysis, We have used
$N_c = 300$ with $\Delta \nu_c = 0.1$ MHz.

The measured Visibilities $\mathcal{V}(\mathbf{U}_a, \nu_n)$ can be
expressed as of sum of the HI signal $\mathcal{S}(\mathbf{U}_a,
\nu_n)$ and the noise $\mathcal{N}(\mathbf{U}_a, \nu_n)$, i.e.,
\begin{equation}
\mathcal{V}(\mathbf{U}_a, \nu_n) = \mathcal{S}(\mathbf{U}_a, \nu_n) +
\mathcal{N}(\mathbf{U}_a, \nu_n)
\end{equation}
assuming that foregrounds have been completely removed from the data.

For the Fisher matrix analysis, it is of convenience to decompose the
visibilities $\mathcal{V}(\mathbf{U}_{a}, \nu_n)$ into delay channels
$\tau_{m}$ (Morales 2005) rather than frequency channels $\nu_n$,
i.e.,
\begin{equation}
v(\mathbf{U}_{a}, \tau_m) = \Delta \nu_c \sum_{n=1}^{N_c} \, e^{2 \pi
  i \tau_{m} \nu_{n}} \, \mathcal{V}(\mathbf{U}_{a}, \nu_n)
\end{equation}
where $\tau_m$ is the delay channel which is defined as follows, i.e.,
\begin{equation}
\tau_m = \frac{m}{B} \hspace{0.5cm} \text{with} \hspace{0.5cm}
\frac{N_c}{2} < m \leq \frac{N_c}{2}
\label{eq:tau}
\end{equation}

The visibilities $v(\mathbf{U}_{a}, \tau_m)$ and $v(\mathbf{U}_{b},
\tau_n)$ are uncorrelated for $m \neq n$ (Paper II).  It is therefore
necessary to only consider the visibility correlations with $m = n$
for which we define the visibility covariance matrix
\begin{equation}
  C_{ab}(m) = \langle v(\mathbf{U}_{a}, \tau_m) v^{*}(\mathbf{U}_{b},
  \tau_m) \rangle \,.
\end{equation}
The visibility covariance matrix $C_{ab}(m)$ can be expressed in terms
of the redshifted HI 21-cm brightness temperature power spectrum
$P_{T}(\mathbf{k}_{\perp}, k_{\parallel})$ as (eq. (5) of Paper II)
\begin{align}
& C_{ab}(m) = \frac{B}{r_{\nu}^2 r_{\nu}^{'}} \left(\frac{2
    k_B}{\lambda^2}\right)^2 \int d^2 U^{'} \tilde{A}({\bf U}_a-{\bf U}^{'})
  \tilde{A}^{*}({\bf U}_b-{\bf U}^{'}) \nonumber \\ & \times
  P_{T}(\mathbf{k}_{\perp}, k_{\parallel}) + \frac{2 \Delta \nu_c B
    \sigma_N^{2}}{(264-a)}\delta_{a,b}
\label{eq:cov}
\end{align}
where the first and the second terms refer to the signal and noise
covariance respectively. Here $r_{\nu}$ is the co-moving distance
between the observer and the region of space from where the HI
radiation originated, $r^{'}_{\nu}=\frac{dr_{\nu}}{d \nu}$ gives the
conversion factor from frequency to co-moving distance ($r_{\nu} =
6.85$ Gpc and $r_{\nu}^{'} = 11.5$ Mpc MHz$^{-1}$ for OWFA) and
$\tilde{A}(\mathbf{U})$ is the Fourier transform of the OWFA primary
beam pattern (eq. (6) of Paper I)). The factor $\frac{2
  k_B}{\lambda^2}$ gives the conversion from brightness temperature to
specific intensity (where $k_{B}$ is the Bultzmann constant),
$P_{T}(\mathbf{k_{\perp}}, k_{\parallel})$ is the redshifted HI 21-cm
brightness temperature power spectrum, $\mathbf{k_{\perp}} = \pi
(\mathbf{U}_a + \mathbf{U}_b)/r_{\nu}$ and $k_{\parallel} = 2 \pi
\tau_m/r_{\nu}^{'}$ respectively refer to the perpendicular and
parallel components of the wavevector $\mathbf{k}$ with $k =
\sqrt{k_{\perp}^2 + k_{\parallel}^2}$ (Bharadwaj, Sarkar \&
  Ali 2015). The rms. noise of the measured visibilities has
  the contribution from the system noise and has a value $\sigma_N =
  6.69 \, {\rm Jy}$ for $16 \, {\rm s}$ integration time (Table 1 of
  Paper I) and the factor $(264-a)^{-1}$ in the noise contribution
  accounts for the redundancy in the baseline distribution for OWFA.

For OWFA, the visibilities at any two baselines $\mathbf{U}_a$ and
$\mathbf{U}_b$ are uncorrelated ($C_{ab}(m) = 0$) if $|a-b| > 1$
ie. the visibility at a particular baseline $\mathbf{U}_a$ is only
correlated with the visibilities at the same baselines or the adjacent
baselines $\mathbf{U}_{a \pm 1}$.  Thus, for a fixed $m$, $C_{ab}(m)$
is a symmetric, tridiagonal matrix where the diagonal represents the
visibility correlation at the same baseline whereas the upper and
lower diagonals represent the visibility correlation between the
adjacent baselines. Figure 1 of Paper II shows the signal contribution
for the diagonal and off-diagonal terms of $C_{ab}(m)$.  The
covariance at adjacent baselines is approximately one fourth of the
covariance at the same baselines.  Further, the noise contributes only
to the diagonal terms and it does not figure in the off-diagonal
terms.

We have used the Fisher matrix (eq. (8) of Paper II)
\begin{equation}
F_{\alpha \gamma} = \frac{1}{2} \sum_m C^{-1}_{ab}(m)
[C_{bc}(m)]_{,\alpha} C^{-1}_{cd}(m) [C_{da}(m)]_{,\gamma}
\label{eq:fisher}
\end{equation}
to predict the accuracy with which it will be possible to constrain
the value of various parameters using observations with OWFA.  The
indices $\alpha,\gamma$ here refer to the different parameters whose
values we wish to constrain. The inverse of the Fisher matrix
$F_{\alpha \gamma}$ provides an estimate of the error-covariance
(Dodelson 2003) for these parameters.  In eq. (\ref{eq:fisher}), the
indices $a,b,c,d$ are to be summed over all baselines.  We have used
eq. (\ref{eq:cov}) to calculate the data covariance matrix $C_{ab}(m)$
and also its derivatives $[C_{ab}(m)]_{,\alpha}$ with respect to the
parameters whose values we wish to constrain.  A discussion of the
parameters considered for the present analysis follows in the next
section.

\section{Modelling and Binning the HI power spectrum}
The redshifted HI 21-cm brightness temperature power spectrum
$P_{T}(\mathbf{k})$ is the quantity that will be directly measured by
any cosmological 21-cm experiment. This quantifies the fluctuations in
the brightness temperature originating from two different sources -
1. the intrinsic fluctuations of the HI density in real co-moving
space and 2. the peculiar velocities which introduce brightness
temperature fluctuations through redshift space distortion. For the
purpose of this work, we have modelled $P_{T}(\mathbf{k})$ as
\begin{equation}
 P_{T}(\mathbf{k}) = (1 + \beta \mu^2)^2 P_{T}^r(k)
\end{equation}
where $P_{T}^r(k)$ is the power spectrum of the HI 21-cm brightness
temperature fluctuations in real space and the factor $(1 + \beta \mu^2)^2$
quantifies the the effect of linear redshift space distortion due to
peculiar velocities (Kaiser 1987; Bharadwaj, Nath \& Sethi 2001; Ali
\& Bharadwaj 2014). Here $\beta$ is the redshift space distortion
parameter and $\mu = k_{\parallel}/k$.

OWFA will probe the $k_{\perp}$ and $k_{\parallel}$ - range $1.9
\times 10^{-3} \leq k_{\perp} \leq 5 \times 10^{-1}$ Mpc$^{-1}$ and
$1.8 \times 10^{-2} \leq k_{\parallel} \leq 2.73$ Mpc$^{-1}$
respectively, thereby covering the $k$-range $ 1.82 \times 10^{-2}
\leq k \leq 2.73$ Mpc$^{-1}$. The present work focuses on making
predictions for the accuracy with which it will be possible to measure
$P_{T}^r(k)$ using OWFA. For this purpose, we have divided the entire
$k$-range probed by OWFA into 20 equally spaced logarithmic $k$-bins,
and we use $k^i$ and $[P^r_{T}]^i$ (with $1 \leq i \leq 20)$ to refer
respectively to the average $k$ and $P_{T}^r(k)$ value for each bin.
We have used $\ln ([P_{T}^r]^i)$ and $\ln (\beta)$ as the parameters
for the Fisher matrix analysis (eq. (\ref{eq:fisher})) which gives an
estimate of the precision with which it will be possible to
measure these parameters.

\section{Results and Discussions}
We need a fiducial model for the $P_{T}^r(k)$ and $\beta$ to carry out
the Fisher matrix analysis. We model the $P_{T}^r(k)$ assuming that it
traces the underlying matter power spectrum $P(k)$ with a linear bias
$b_{\rm HI}$ as also assumed by Bharadwaj, Nath \& Sethi (2001),
Bharadwaj \& Sethi (2001), Wyithe \& Loeb (2009),
\begin{equation}
P^r_{T}(k) = (\bar{x}_{\rm HI} \, b_{\rm HI} \, \bar{T})^2 \, P(k)
\label{eq:PHIr}
\end{equation}
where $\bar{x}_{\rm HI}$ is the mean neutral hydrogen fraction. The
characteristic HI brightness temperature $\bar{\rm T}$ is defined as
(Bharadwaj \& Ali 2005)
\begin{equation}
\bar{T}(z) = 4.0\,\text{mK} \, (1+z)^2 \, \left( \frac{1-Y_P}{0.75}
\right) \, \left( \frac{\Omega_b h^2}{0.020} \right) \left(
\frac{0.7}{h} \right) \left( \frac{H_0}{H(z)} \right)
\label{eq:Tbar}
\end{equation}
where $Y_P$ is the helium mass fraction and the other symbols
  in the above equation have their usual meanings.

The parameter $\beta$ in the observed $P_T(k)$ (eq. \ref{eq:PHIr}) is
defined as $\beta = f(\Omega)/b_{\rm HI}$ where $f(\Omega)$ quantifies
the growth rate of the matter density perturbations, whose value is
specified by the background $\Lambda$CDM cosmological model. Note that
the various terms used in eq. (\ref{eq:PHIr}) correspond to the
redshift, $z = 3.35$ where HI radiation originated.

We have used $\bar{x}_{\rm HI} = 0.02$ for our analysis which
  corresponds to the neutral gas mass density parameter $\Omega_{\rm
    gas} = 10^{-3}$. This value of $\Omega_{\rm gas}$ comes from DLA
  observations in the redshift range of our interest (Prochaska \&
Wolfe 2009; Noterdaeme et al. 2012; Zafar et al. 2013).  Simulations
(Bagla, Khandai \& Datta 2010; Guha Sarkar et al. 2012; Sarkar,
Bharadwaj \& Anathpindika 2016) and analytical modelling (Marin et
al. 2010) suggest the use of a constant, scale-independent bias at
wave numbers $k \leq 1$ Mpc$^{-1}$, and we use the value $b_{HI}=2.0$
for our entire analysis. We use these values and the cosmological
parameters to calculate the fiducial values of $[P_{T}^r]^i$ (pointsin Figure
\ref{fig:err}) and $\beta = 4.93 \times 10^{-1}$.

The value of  $\beta$ can be estimated by sampling the Fourier modes
$\mathbf{k}$ with a fixed magnitude $k$ which are, however, oriented at
different directions to the line-of-sight. In other words, $\mu =
k_{\parallel}/k$ should uniformly span over the entire range $-1 \leq
\mu \leq 1$. The minimum value of $k_{\parallel}$ probed
  by OWFA is approximately $10$ times larger than the minimum
  value of  $k_{\perp}$. The maximum value of $k_{\parallel}$
  is also $\sim 4$ times larger than  the maximum value of
  $k_{\perp}$ (Table II of Paper II). In addition to this, the
  sampling width for $k_{\parallel}$ is roughly $\sim 20$ times
  larger than  that of $k_{\perp}$. These disparities  lead to a non-uniform
  distribution where the  $\k$  modes are largely concentrated around $\mu =
  1$ (see Figure 3 of Paper II). This anisotropic distribution of
  the $\k$ modes does not make OWFA very suitable for measuring $\beta$,
  and we do not consider this  in our  analysis.

We have considered two different cases for error predictions. In the
first situation, we consider the Conditional errors $\sigma_{ic}$ for
the measurement of the binned HI power spectrum
$[P_{T}^r]^i$. The conditional error $\sigma_{ic}$ represents the
  error on the measurement of $[P_{T}^r]^i$ in a situation
where the values of all the other
  parameters   are precisely known. Here, we calculate $\sigma_{ic}$ for the
$i$-th bin by assuming that the values of $\beta$ and $[P_{T}^r]^j$
are precisely known for all the other bins. We use $\sigma_{ic} =
1/\sqrt{F_{ii}}$ to compute the conditional error for the $i$-th bin.

In the second situation, we have considered the Marginalized errors
$\sigma_{im}$ for the measurement of
$[P_{T}^r]^i$. The marginalized error $\sigma_{im}$ gives the
  error on the measurement of $[P_{T}^r]^i$ without assuming any
  prior information about the other parameters. While estimating the
error for the $i$-th bin, we have marginalized over the values of $\beta$ and
$[P_{T}^r]^j$ in the  other bins. In our previous work (Paper II), we have
calculated the marginalized error on the measurement of the amplitude
of the HI power spectrum with a prior on $\beta$ in the range $0.329
\leq \beta \leq 0.986$. In the present work, we have not imposed any
prior on $\beta$ and we have marginalized $\ln ([P_{T}^r]^i)$ and $\ln
(\beta)$ over the entire range $-\infty$ to $+\infty$. We use
$\sigma_{im} = \sqrt{[F^{-1}]_{ii}} $ to calculate the marginalized
error for the $i$-th bin. The conditional  and the marginalized
  errors  here represent the two limiting cases, and  the
  error estimates would lie somewhere in between  $\sigma_{ic}$ and
  $\sigma_{im}$  if we impose priors on the value of $\beta$  or any of  the
  other parameters.

In Paper II, we have shown that a $5\sigma$ detection of the amplitude
of the $P_{T}^r$ is possible with $\sim 150$ hours of observations.
We therefore need to consider an observing time $t > 150$ hours for
measuring the $[P_{T}^r]^i$ in different $k$-bins. Figure
\ref{fig:sigma} shows both the conditional ($\sigma_{ic}$) and
marginalized ($\sigma_{im}$) errors for $1000$ hours of
observation. Here $\sigma_{ic}$ and $\sigma_{im}$ are respectively the
conditional and marginalized errors for different $\ln([P^r_T]^i)$ which are
the parameters for the Fisher matrix analysis. Here $\sigma_{ic}$ and
$\sigma_{im}$  represent the two
limiting cases for the error estimates. We expect the error estimates to lie
between these two limiting values in case we impose a prior on the
value of $\beta$ (Paper II).

\begin{figure}
\begin{center}
\psfrag{Conditional}[c][c][0.8][0]{Conditional $\sigma_{ic}$}
\psfrag{Marginalized}[c][c][0.8][0]{Marginalized $\sigma_{im}$}
\psfrag{p3}[c][c][1.0][0]{$\qquad 1,000$ hours}
\psfrag{p2}[c][c][1.2][0]{{Fractional error}}
\psfrag{p1}[c][c][1.2][0]{$k$ Mpc$^{-1}$}
\vskip.2cm \centerline{\hspace{-1.5cm}{\includegraphics[scale
      =.80]{sigma.ps}}}
\caption{The figure shows the fractional errors for the
    measurement of $\ln([P_{T}^r]^i)$ in different $k$-bins with
    $1,000$ hours of observation for two situations, conditional
    $\sigma_{ic}$ (red solid line) and marginalized $\sigma_{im}$
    (green dashed line).}
\label{fig:sigma}
\end{center}
\end{figure}

We find that the values of $\sigma_{ic}$ and $\sigma_{im}$ agree within
$15\%$, except at the $k$-bins lying in the range $0.06 \leq k \leq 0.3$
Mpc$^{-1}$ where the difference is $\sim 20-35\%$. This
suggests that $\sigma_{ic} = 1/\sqrt{F_{ii}}$ and $\sigma_{im} =
\sqrt{[F^{-1}]_{ii}}$ are not significantly different, indicating that
the contribution from the off-diagonal terms of  $F_{ij}$ are
small. We therefore conclude that the measurements of  $P_{T}^r$ in
different $k$-bins are by and large uncorrelated. In the subsequent
analysis, we have used $\sigma_{ic}$ for predicting errors on the
measurements of $[P_{T}^r]^i$ in different $k$-bins.

\begin{figure}[h]
\begin{center}
\psfrag{k1}[c][c][1.2][0]{$P_T^r(k)$ Mpc$^{3}$ mK$^{2}$}
\psfrag{k2}[c][c][1.2][0]{$k$ Mpc$^{-1}$} \psfrag{1000
  hr}[c][c][1.0][0]{$1,000$ hours}
\vskip.2cm
\hspace*{-1.5cm}\centerline{{\includegraphics[scale
      =.80]{err_bin.ps}}}
\caption{The binned HI power spectrum $[P_{T}^r]^i$ (points) with
  $1\sigma$ errors (vertical bars) for $1,000$ hours of observation. }
\label{fig:err}
\end{center}
\end{figure}

Figure \ref{fig:err} shows the binned HI power spectrum $[P_{T}^r]^i$
with the $1\sigma$ errors $\Delta [P_{T}^r]^i = \sigma_{ic} \times
[P_{T}^r]^i$ for $1,000$ hours of observation . The error $\Delta
[P_{T}^r]^i$ on the measurement of the $P_{T}^r$ in a given $k$-bin is
the combination of contributions from the system noise and the cosmic
variance. The noise term in eq.(\ref{eq:cov}) is suppressed by the
factor $(264-a)^{-1}$ due to the redundancy of the OWFA baselines. We
see that the noise contribution goes up as the baseline number $a$ is
increased. The small $k$-bins which correspond to small baselines,
have smaller noise contribution than the larger $k$-bins which
correspond to large baselines. Here we have used logarithmic binning
where the bin width and the number of $k$-modes in a bin increase with
$k$. The cosmic variance in a given $k$-bin goes down with number of
$k$-modes in that bin. We therefore expect the cosmic variance to be
maximum at the smallest $k$-bin and decrease with increasing $k$. As a
whole the errors at smaller $k$-bins are dominated by the cosmic
variance whereas at larger $k$-bins, the errors are dominated by the
system noise.

We can see from Figure \ref{fig:sigma} that $\sigma_{ic}=\Delta
[P_{T}^r]^i/[P_{T}^r]^i$, which is the relative error on the binned
power spectrum, is minimum in the range $k \sim 0.1 - 0.2 \, {\rm
  Mpc}^{-1}$. The cosmic variance dominates the relative error at
smaller values of $k$ $(< 0.1\, {\rm Mpc}^{-1}) $ whereas the system
noise dominates at larger $k$ values $(>0.2 \, {\rm Mpc}^{-1}) $.  We
also see that the relative error is lower than $0.2$ in the range
$0.05 \leq k \leq 0.3 \, {\rm Mpc}^{-1}$ where our results predict a
$5 \sigma$ detection of the binned power spectrum (Figure
\ref{fig:err}).

\begin{figure}
\begin{center}
\psfrag{k2}[c][c][1.5][0]{$t$ hours} \psfrag{k1}[c][c][1.5][0]{$k$
  Mpc$^{-1}$} \psfrag{k3}[c][c][1.5][0]{SNR}
\psfrag{Ten}[c][c][1][0]{$\mathbf{10 \sigma}$}
\psfrag{sev}[c][c][1][0]{$\mathbf{7 \sigma}$}
\psfrag{fiv}[c][c][1][0]{$\mathbf{5 \sigma}$}
\psfrag{thr}[c][c][1][0]{$\mathbf{3 \sigma}$}
\vskip.2cm
\centerline{{\includegraphics[angle=-90,scale=1.0]{cont.ps}}}
\caption{The SNR contours as function of $k$-bin and observations time
  $t$.}
\label{fig:cont}
\end{center}
\end{figure}

We have so far considered the errors on the measurement of
$[P_{T}^r]^i$ with a given hours of observing time ($1,000$ hours). We
shall now try to understand how the errors $\sigma_{ic}$ vary with
observation time $t$. The time dependence of the visibility covariance
$C_{ab}(m)$ (eq. (\ref{eq:cov})) comes in through the rms. noise of
the measured visibilities $\sigma_N$ which scales inversely with
$\sqrt{t}$, ie. $\sigma_N \sim 1/\sqrt{t}$. We expect the visibility
covariance $C_{ab}(m)$ to vary inversely with $t$, ie. $C_{ab}(m) \sim
1/t$ for small observing times where the noise contribution is
considerably larger than the signal, and we expect $C_{ab}(m)$ to have
a constant value, independent of the observing time, for large values
of $t$.  The derivatives of the $C_{ab}(m)$ which appear in the Fisher
Matrix (eq. (\ref{eq:fisher})) are independent of $t$. It then follows
that the Fisher matrix $F_{\alpha \gamma}$ scales as $F_{\alpha
  \gamma} \sim t^2$ for small observation times and $F_{\alpha
  \gamma}$ has a constant value for large $t$.  We therefore expect
the relative errors $\sigma_{ic}$ to vary as $\sigma_{ic} \sim 1/t$
for small observing times, and become independent of $t$ for large
observation times where the error is dominated by the cosmic variance.

Figure \ref{fig:cont} shows a contour plot of the Signal-to-Noise
Ratio (SNR)
\begin{equation}
\text{SNR} = \frac{1}{\sigma_{ic}} = \frac{[P_{T}^r]^i}{\Delta
  [P_{T}^r]^i},
\end{equation}
as functions of the Fourier mode $k$ and observation time $t$.  We see
that a statistically significant measurement ( $3\sigma$) of the
binned power spectrum is only possible for observations times greater
than $200 \, {\rm hours}$.  A $3\sigma$ detection of $[P_{T}^r]^i$ is
possible in the $k$-range $0.04 \leq k \leq 0.2$ Mpc$^{-1}$ with $200
- 300$ hours of observation. Detection at a significance of $5\sigma$
is not possible with $t \leq 500$ hours of observation. We find that a
$5\sigma$ detection of $[P_{T}^r]^i$ is possible for $0.05 \leq k \leq
0.3$ Mpc$^{-1}$ with $1,000$ hours of observing time. Note that the
SNR peaks in the range $k \sim 0.1 - 0.2$ Mpc$^{-1}$.  In this $k$
range the SNR continues to increase with $t$ for the entire $t$ range
shown here and a $10 \sigma$ detection is possible with $2,000$ hours
of observation. At $k < 0.1 \, {\rm Mpc}^{-1}$, the SNR stops
increasing with $t$ beyond a certain point.  The SNR here becomes
dominated by the cosmic variance as $t$ is increased, and the SNR
contour becomes parallel to the $t$ axis. We see that
  irrespective of the observing time, a $5 \sigma$ detection is not
  possible for $k < 0.036 \, {\rm Mpc}^{-1}$ if only one pointing is
  considered. For $k > 0.2 \, {\rm Mpc}^{-1}$ the error is system
noise dominated, and the SNR continues to increase with increasing
$t$. However, we see that a $5 \sigma$ detection is not possible for
$k > 0.5 \, {\rm Mpc}^{-1}$ within $2,000$ hours of observation.

\begin{figure}[h]
\begin{center}
\psfrag{p2}[c][c][1.2][0]{SNR} \psfrag{p1}[c][c][1.2][0]{$t$ hours}
\psfrag{k1}[c][c][0.9][0]{\hspace*{-1.5cm}$0.036 \, {\rm Mpc}^{-1}$}
\psfrag{k2}[c][c][0.9][0]{\hspace*{-1.5cm}$0.15 \, {\rm Mpc}^{-1}$}
\psfrag{k3}[c][c][0.9][0]{\hspace*{-1.5cm}$0.33 \, {\rm Mpc}^{-1}$}
\psfrag{k4}[c][c][0.9][0]{\hspace*{-1.5cm}$1.16 \, {\rm Mpc}^{-1}$}
\vskip.2cm \centerline{{\includegraphics[scale=1.0]{snr.ps}}}
\caption{The Signal-to-Noise Ratio (SNR) with observation time $t$ for
  different $k^i$ values (mentioned in the figure).}
\label{fig:snr}
\end{center}
\end{figure}

As mentioned earlier, we expect SNR $\propto\, t$ for small observing
times when the error is system noise dominated, and we expect the SNR
to saturate at a fixed value for large observing times where the
cosmic variance dominates.  Figure \ref{fig:snr} shows how the SNR
changes with observing time $t$ for a few representative $k$-bins. The
small $k$ bins have a relatively large cosmic variance.  We see that
the SNR at the smallest $k$ bin ($0.036 \, {\rm Mpc}^{-1}$) shown in
this figure is nearly saturated at a very small observing time ($t
\sim 300$ hours), and increases very slowly for larger observing
times.  A $5 \sigma$ detection in this bin requires $\sim 10,000$
hours of observation.  The $k$-bin at $0.33 \, {\rm Mpc}^{-1}$ shows
the ${\rm SNR} \propto t$ scaling for $t \le 700 \, {\rm hours}$,
beyond which the increase in SNR is slower. The two larger $k$-bins
shown in the figure show the ${\rm SNR} \propto t$ behaviour over the
entire $t$ range considered here. However, note that the largest
$k$-bin with $k^i = 1.16 \, {\rm Mpc}^{-1}$ shown in the figure has a rather low
SNR, and a $5 \sigma$ detection is only possible with $10,000 \, {\rm
  hours}$ of observation.

\begin{figure}[h]
\begin{center}
\psfrag{p2}[c][c][1.2][0]{$t_{\rm CV}$ hours}
\psfrag{p1}[c][c][1.2][0]{$k \, {\rm Mpc}^{-1}$}
\vskip.2cm \centerline{{\includegraphics[scale=1.0]{snr-sp.ps}}}
\caption{The observation time ($t_{\rm CV}$) at which the cosmic
  variance starts to dominate the error on the measurement of the HI
  power spectrum for different $k$-bins.}
\label{fig:snrsp}
\end{center}
\end{figure}

As mentioned earlier, we expect the SNR to increase with time
  $t$, ie. ${\rm SNR} \propto t$ for small observing times. The
  increase in the SNR slows down for larger observing times, and for
  even larger observing times $(t \ge t_{\rm CV})$ the SNR saturates
  at a fixed value which is determined by the cosmic variance in the
  particular $k$-bin.  Here $t_{\rm CV}$ referes to the observing time
  beyond which the SNR is determined by the cosmic variance, and we
  have estimated this for the different $k$ bins such that the SNR
  increases slower than $t^{0.002}$ for $(t \ge t_{\rm CV})$. Figure
  \ref{fig:snrsp} shows $t_{\rm CV}$ for the different $k$-bins. For
  any particular bin, it is not possible to increase the SNR any
  further by increasing the observing time beyond $t_{\rm CV}$. We
  find that $t_{\rm CV}$ increases approximately as $t_{\rm CV}
  \propto k^{0.63}$ for $k \leq 1.0 \, {\rm Mpc}^{-1}$. The increase
  in the $t_{\rm CV}$ is rather slow for $k \geq 1 \, {\rm Mpc}^{-1}$
  and saturates at $t_{\rm CV} \sim 15000 \, {\rm hr}$ beyond $k = 2.0
  \, {\rm Mpc}^{-1}$. This behaviour is decided by a combination of
  several factors including the OWFA baseline redundancy, the sampling
  of the 3D Fourier modes and the logarithmic binning.

The discussion till now has entirely focused on observations
  in a single field of view. As already mentioned, the ${\rm SNR}$
  ceases to increase with observing time once $t \sim t_{\rm CV}$. We
  see that $t_{\rm CV} \sim 1,000 \, {\rm hr}$ at the smallest $k$
  bin. The ${\rm SNR}$ in this bin will saturate for $t > 1,000 \,
  {\rm hr}$ and it is necessary to observe multiple fields of view to
  increase the ${\rm SNR}$ any further. The ${\rm SNR}$ scales as
  ${\rm SNR} \propto \sqrt{N}$, where $N$ is the number of fields of
  view.  A possible observational strategy for OWFA would be to
  observe multiple fields of view, with each field being observed for
  a duration of $1,000 - 2,000 \,{\rm hr}$. The $3 \sigma$ contour in
  Figure \ref{fig:cont} would correspond to $5.2 \sigma$ for
  observations in $N=3$ fields of view.  We see that a $5 \sigma$
  detection is possible in nearly all the $k$ bins if $3$ fields of
  view are observed for $1,500 \, {\rm hr}$ each.

\section{Summary and Conclusions}
We have considered Phase II of OWFA to study the prospects of
measuring the redshifted 21-cm power spectrum in different $k$-bins.
The entire analysis is restricted to observations in a single field of
view.  We find that a $5 \sigma$ detection of the binned power
spectrum is possible in the $k$ range $0.05 \leq k \leq 0.3 \, {\rm
  Mpc}^{-1}$ with $1,000$ hours of observation.  The ${\rm SNR}$ peaks
in the $k$ range $0.1 - 0.2 \, {\rm Mpc}^{-1}$ where a $10 \sigma$
detection is possible in $2,000$ hours of observation.  Our study
reveals that it is not very advantageous to observe much beyond
$1,000$ hours as the error in measuring the power spectrum become
cosmic variance dominated in several of the small $k$-bins, and the
${\rm SNR}$ in these bins increase rather slowly with increasing $t$.

As discussed earlier, the variation of the baseline over the observing
bandwidth is $\sim 5\%$. This makes both the diagonal and off-diagonal
components of the Fisher matrix to change, which is expected to be not
more than $5-10\%$.

The redshifted 21-cm signal provides an unique way to measure the BAO
in the post-reioinization era ($z \leq 6$).  This is perceived to be a
sensitive probe of the dark energy. The BAO is a relatively small
feature ($\sim 10 - 15 \%$) that sits on the HI power spectrum. The
five successive peaks of the BAO span the $k$ range $0.045 \leq k \leq
0.3$ Mpc$^{-1}$, which is well within the $k$-range probed by OWFA.
The detection of the BAO requires measuring
the HI power spectrum at a significance of $50\sigma$ or more. From
Figure \ref{fig:cont}, we find that such a sensitivity cannot be
achieved in the relevant $k$ range within $t \sim 2000$ hours of
observation. It is also clear that the required sensitivity cannot be
achieved by considering observations in a few fields of view.  For
detecting the BAO it is necessary to consider a different
observational strategy covering the entire sky (e.g. Shaw et
al. 2013). We plan to address this in future work.

\section*{Acknowledgement}
The authors acknowledge Jayaram N. Chengalur, Jasjeet S. Bagla,
Tirthankar Roy Choudhury, C.R. Subrahmanya, P.K. Manoharan and
Visweshwar Ram Marthi for helpful discussions. AKS would like to
acknowledge Rajesh Mondal and Suman Chatterjee for their help. AKS
would like to specially mention Debanjan Sarkar for a detailed reading
of the manuscript and providing important suggestions. AKS would also
like to express thanks to the anonymous referees whose critical
suggestions helped towards a major improvement of the language and
presentation of the manuscript. SSA would like to acknowledge CTS, IIT
Kharagpur for the use of its facilities and thank the authorities of
IUCAA, Pune, India for providing the Visiting Associateship programme.

redpajama_set_name: RedPajamaArXiv


Comfeel Plus Transparent Dressings are a Non-Adhesive, thin, flexible Hydrocolloid dressing with a semi permeable polyurathane top film. When it comes into contact with wound exudate, it forms a viscous gel that absorbs exudate, but does not adhere to the wound. The transparency and printed grid aids wound measurement.
Wounds with no or low exudate. Pressure ulcers, leg ulcers, superficial burns, superficial partial-thickness burns, donor sites, postoperative wounds, skin tears and skin abrasions. Use also as a protection on epithelialised tissue or as a secondary dressing.
Patients with known sensitivity to one of the ingredients.


text:
Media advisory: UN gathering to call for a stronger multilateral approach to deliver on the Beijing Platform for Action – the blueprint for advancing gender equality
Robust and urgent actions must bring transformative change to women and girls' empowerment
10:00 am to 5:00 pm EDT
Live-streamed at http://webtv.un.org
Member states and observers, civil society organizations, gender equality leaders, CEOs, and heads of academia will gather virtually on 21 July 2020 in a multi-stakeholder hearing to bolster priority actions at the global and national level that will address the challenges that threaten the bold vision of the Beijing Declaration and Platform for Action, 25 years after its adoption.
The Beijing Declaration and Platform for Action
The Beijing Declaration and Platform for Action remains today the most comprehensive and transformative global agenda for the achievement of gender equality and the empowerment of women and girls. Since its adoption, significant progress has been made on women and girls' rights, however the UN Secretary-General's report on the Review and appraisal of the implementation of the Beijing Declaration and Platform for Action, and UN Women's report, "Women´s Rights in Review 25 years after Beijing" warned that despite many advances, progress towards gender equality has been faltering and hard-won advances are being reversed today.
Multi-stakeholder hearing
"By working together- girls and boys, women and men- we can galvanize multilateral action to realise human rights of all women and girls," said the President of the UN General Assembly Tijjani Muhammad-Bande in a video message to commemorate this year's International Women's Day.
Mr. Muhammad-Bande, with the support of UN Women, is convening an interactive hearing to call for a stronger multilateral commitment to implement the Beijing Platform for Action to advance the rights of women and girls, intensify efforts to build back better from the pandemic and set the stage for the High-Level Meeting of the UN General Assembly on the margins of the High-Level Week, under the theme "Accelerating the realization of gender equality and the empowerment of women and girls". The virtual gathering on 21 July will provide an opportunity for all stakeholders to exchange experiences, lessons learned and good practices to advance the full, effective and accelerated implementation of the Beijing Declaration and Platform for Action.
"It's up to us to make sure that we use the power of multilateral investment and commitment to realize the potential gains from radical, positive action to redress long-standing inequalities in multiple areas of women's lives," said UN Women Executive Director Phumzile Mlambo Ngcuka. "I ask governments and all other service providers including the private sector to take this opportunity to plan their response to COVID-19 as they have never done before, include women in its design, and fully take a gender perspective into account," she added.
COVID-19 has laid bare pre-existing inequalities. Across every sphere, from health to the economy, security to social protection, women and girls are disproportionately affected.
While women's political representation has doubled since 1995, men still control more than three quarters of the seats in the single and lower houses of parliaments around the world.
Nearly a billion women and girls 15 years and over lacked basic reading and writing skills in 2018.
Women 25 to 34 years old are 25% more likely than men to live in poverty.
It is the most marginalized women who have least contributed to the climate crisis who are most affected by environmental degradation and natural disasters.
After years of progress, the proportion of peace agreements that included references to women dropped from 32 per cent between 2011 and 2015 to 7.7 per cent in 2018.
On the 25th anniversary of the Beijing Platform for Action, the progress review of this visionary agenda takes place for the first time in the context of the 2030 Agenda for Sustainable Development and its Sustainable Development Goals (SDGs). The 2030 Agenda, including SDG 5 on achieving gender equality and empowering all women and girls, highlighted the centrality of gender equality to progress across all the Goals and targets.
The Decade of Action for the Sustainable Development Goals, called for by world leaders at the SDG Summit in 2019, recognized the value in strengthening international cooperation to tackle both emerging and existing gaps in the realization of gender equality and the empowerment of all women and girls. In addition to a stronger multilateral approach, priority actions for advancement of gender equality include: repealing discriminatory laws, the provision of adequate financing, closing gender data gaps, harnessing the potential of technology and innovation and eliminating gender stereotypes.
To view the multi-stakeholder hearing, watch on UN Webcast: http://webtv.un.org
For more information, visit:https://www.un.org/pga/74/event/accelerating-the-realization-of-gender-equality-and-the-empowerment-of-all-women-and-girls/
Full Programme: https://www.un.org/pga/74/wp-content/uploads/sites/99/2020/07/Programme-MSH-on-21-July.version-9-July.pdf
Hashtags: #GlobalGoals, #GenerationEquality
Available for Interviews:
President of the UN General Assembly Tijjani Muhammad-Bande
UN Women Executive Director Phumzile Mlambo-Ngcuka (by request)
UN Women: Media.team[at]unwomen.org
Office of the President of the UN General Assembly: kling[at]un.org
Watch archived webcast
Ana Šaćipović: Building a bridge between two worlds

redpajama_set_name: RedPajamaCommonCrawl


text:
Halton seeks support to develop internships offer
Halton Borough Council wish to engage a service to build on work undertaken so far, to ensure that Halton can make available an appropriate offer of Supported Internships for young people age 16-25.
The Council wishes to achieve the following outcomes:
Call for evidence: Supporting inclusive workplaces for everyone
ERSA has issued a call for evidence about Supporting inclusive workplaces for everyone – Health Related Pathways to Work
A Health and Wellbeing Alliance project, led by Homeless Link and Win/Win Alliance involving ERSA and Making Every Adult Matter (MEAM), is supporting Public Health England (PHE)'s Health and Work team to work towards inclusive workplaces for everyone.
Learning disability and autism a national clinical priority for NHS
Autism and learning disability have been named as one of the 4 clinical priorities for long term planning within the NHS.
On 18th June the Prime Minister set out a funding settlement for the NHS in England for the next five years. In return, the NHS has been asked to set out a long term plan for the future of the NHS by Autumn, setting out its ambitions for improvement over the next decade, and its plans to meet them over the five years of the funding settlement.
Greater Manchester sets learning disability employment target
Greater Manchester has set a target of achieving 7% employment rates for people with learning disabilities across all of the Greater Manchester boroughs by 2020. The target is included within its GM Learning Disability Strategy and flagged up in a letter to all authorities in the region.
The letter, from Lord Smith of Leigh, the Chair of Greater Manchester Health and Care Board, states:
South Yorkshire starts major IPS trial
A £7.9m pilot has been officially launched to help South Yorkshire people with disabilities and health conditions to stay in employment and rejoin the workforce. The 'Working Win' scheme aims to assess the best type of support for those who are out of work, or struggling in employment due to health problems.
Work experience opportunities at Channel 4
Channel 4 is seeking applications for their 4Talent work experience programme. They have a variety of departments involved this time around including Content Management, Sales, Film4, Legal and Commissioning.
Consultation on support for ex-offenders
The Ministry of Justice has issued a Call for Evidence to improve their understanding of:
1. Inclusive Recruitment Practices
What are employers doing, if anything, to create fair opportunities for ex-offenders to compete for jobs within their organisations in the UK?
What information or support would help employers to make the decision to remove the criminal conviction declaration tick-box from their job application forms?
Ethical warehouse space to rent in London
The Camden Society's fulfilment and distribution social enterprise, Mailout, has 787 square feet of warehouse space available to rent in Central London from August 2018. The Camden Society is looking for an ethically minded partner who would like to take advantage of a great storage and work space in Kentish Town and who is excited by the prospect of offering opportunities to people they support.
Please see the attachment for further details.
Consultation on Work & Health Programme statistics
From late autumn 2018, the Department for Work and Pensions (DWP) plans to release regular experimental statistics about the Work and Health Programme (WHP). These will provide information about the number of:
NDTi announces new Chief Executive
NDTi has announced the appointment of Paul Marshall as the new Chief Executive of the National Development Team for Inclusion (NDTi).
Paul has nearly 20 years' experience in leading social change and joins NDTi from Liverty, one of the country's largest social housing providers, where he was Director of Community Engagement. He previously worked in local government and housing in the North East, driving inclusion, community benefit, service transformation and decentralsation.


text:
Five Things You Need to Know About Third Party Risk in 2022
It's no longer enough to simply ensure that your organization's systems and enterprise web presence are secure. Your risk management program needs to look beyond the perimeter of your organization to properly vet the third and fourth-party vendors who will have access to your data without being subject to your internal risk management process. The use of third parties in your supply chain or for data handling create potential risks that can be compounded by these third-party weaknesses. The 2013 Target data breach, which began at an air conditioning subcontractor, is a well known example, but the danger of third-party vendor risk has only increased. More third party breaches are being discovered than ever before. The discipline of third-party risk management (or TPRM) has evolved to help manage this new type of risk exposure.
Here are five key things to know about vendor risk:
1. Risk Starts Small
If an attacker is going to target a large organization, they'll want an entry point that won't raise suspicion. This means using a valid entry point that they can access while masked as a legitimate user. The attacker finds a third party that is less secure– often a smaller vendor with less stringent security protocols. They then leverage this access to break into a higher value organization. For example, in the Target breach, attackers began by using malware to steal credentials from the air conditioning subcontractor, and from there had access to Target's vendor-dedicated web services.
2. Risk Extends Beyond Primary Vendors
The scope of risk is greater than a single third-party relationship would suggest, as an organization's third parties can also have their own third-party vendors, known as fourth-parties, or "second-tier" third-parties. Organizations must understand how their first-tier vendors manage their own third parties. PwC also notes that vendors based overseas come with their own challenges, having "different laws, practices, and business ethics." For example, many companies outside the United States are bound by data sovereignty laws that prevent shipping their citizens' data to the U.S. because of privacy concerns. Third-party risks also don't need to involve hacks or attacks on a vendor. With the increasing use of cloud storage, unsecured cloud instances managed by third parties are a frequent cause of data exposure.
3. Primary Companies Are Held Responsible
For customers, the complexity of third-party relationships can make the full scope of cybersecurity risk difficult to comprehend. Even if a security risk is due to a service provider's lax security, in the mind of the customer it will be the main organization that bears responsibility. This is a legal consideration, too. The organization will often find it difficult to show that it took sufficient steps to manage its third-party risk through due diligence, and will be considered to retain responsibility even if a third party handled its data. There's some justification to this: if a company takes every precaution internally, but fails to conduct due diligence by vetting the security of a vendor using a tool like a cyber risk assessment questionnaire, it may as well have taken no precautions at all.
4. Risk Must Be Mitigated Throughout the Data Lifecycle
Even former third-party relationships can create risk to an organization. For example, TigerSwan's former recruiting vendor left sensitive information publicly available in an S3 bucket until only recently. While the contract with the vendor was terminated in February 2017, thousands of resumes remained stored in the Amazon S3 subdomain "tigerswanresumes." When doing business with third-party vendors, it's important to understand not just how sensitive data will be stored, but also how it will be handled when the business relationship ends.
5. Traditional Cybersecurity Isn't Enough
The Software Engineering Institute states that "[traditional] information security practice sometimes treats third party risk management as an 'add-on' to otherwise siloed security activities." Organizations manage risk areas independently, both internally and for third-party relationships, often by simply reacting to issues as they arise. This quick solution may work in the short term, but given the real-time nature of cyber risk, it fails to provide a complete picture and leaves dangerous levels of risk exposure that can only be controlled through ongoing monitoring. What's necessary, according to Deloitte, is a proactive approach to risk as a source of organizational value. This covers all categories of third-parties and all areas of risk, considering operational risk factors […] with reputational/financial risk factors […] and legal/regulatory risks[…].
Making Resilience a Reality
A fully developed approach to managing third party risk covers the entire organization, addressing both third-party behavior and the relationships within the digital environment. It requires vetting vendors through due diligence processes, the use of vendor risk assessment questionnaires for, enforcement of minimum security standards, and ongoing monitoring of vendors as part of the overall risk management program. Achieving that level of third-party management is challenging. But thanks to technology innovations such as security ratings, and new approaches to the problem, next generation vendor risk management is within reach.
We're seeing sectors such as the financial services industry beginning to lead the charge on managing third-party risk, thanks to the impact of regulatory requirements from entities such as the OCC and Federal Reserve in the US, and APRA in Australia. In a typical financial institution, multiple stakeholders from the board of directors, senior management, enterprise risk managers and internal audit are being mandated to implement robust risk assessment processes and lift their game to tackle this growing problem.
Axel Sukianto
The Buyer's Guide to Third Party Risk Management
Learn about the capabilities you need to understand your third-party risk, manage your vendors, and avoid data breaches.
How to Manage Third-Party Risk in a World of Breaches
A comprehensive overview for managing third-party risk. Learn about common causes of third-party risks and how to mitigate them in this post.
9 Ways to Prevent Third-Party Data Breaches in 2022
This is a complete guide to preventing third-party data breaches. Learn about how organizations like yours are keeping themselves and their customers safe.
What Is Third-Party Risk Management? TPRM Clearly Explained
This is a complete guide to third-party risk management. Learn how to reduce third-party and fourth-party risk with this in-depth post.
Planning Your Vendor Security Assessment Questionnaire [2022 Edition]
Learn the 6 key steps to create effective vendor security assessment questionnaires in 2019, so you can better manage your vendor risk exposure.
How to Prevent Supply Chain Attacks with Honeytokens
Supply chain attacks are on the rise but their attempts could be detected with Honeytokens. Learn how to implement them into your cybersecurity.
Edward Kost


text:
è un videogioco di ruolo della serie Digimon sviluppato da Prope e pubblicato da Bandai il 17 gennaio 2013 per PlayStation Portable esclusivamente in Giappone; il titolo è basato sull'anime omonimo. È il primo gioco prodotto per festeggiare il quindicesimo anniversario del franchise, assieme a Digimon World Re:Digitize Decode e Digimon Crusader usciti successivamente nello stesso anno.

Il gioco narra delle vicende avvenute nella prima serie animata e del film Our War Game!. Dopo aver completato la storia principale del gioco, un episodio originale che presenta i protagonisti delle serie successive potrà essere giocato. Le prime copie del gioco hanno ricevuto in regalo il minigioco Digivice Ver. PSP, il quale emula il Digimon virtual pet e può essere scaricato sulla propria console tramite il servizio online PlayStation Network.

Trama

Come nell'anime del 1999, Digimon Adventure è la storia di sette bambini che durante un campo estivo vengono teletrasportati in una strana dimensione parallela chiamata "Mondo Digitale". I protagonisti sono Tai Kamiya ed i suoi amici Matt Ishida, Sora Takenouchi, Izzy Izumi, Mimi Tachikawa, Joe Kido e TK Takaishi che incontreranno i loro partner Digimon e cercheranno un modo per tornare a casa. Tuttavia, verranno a conoscenza che è presente anche un ottavo bambino prescelto e che devono salvare il loro mondo dai Digimon malvagi.

Modalità di gioco
All'inizio il giocatore potrà controllare sette personaggi ed i loro corrispettivi partner Digimon. Durante il terzo arco narrativo, quello di Myotismon, verrà resa disponibile anche Kari Kamiya assieme a Gatomon. In ogni episodio uno dei personaggi assume il ruolo di leader ed altri due Digimon potranno aiutarlo nelle battaglie. In alcune occasioni verrà chiesto al momentaneo capo del gruppo di parlare con gli altri membri e di scegliere fra due possibili risposte, se il giocatore selezionerà quella corretta aumenterà il livello di Affinità fra i due ragazzi. L'aumento di Affinità porta ad avere diversi benefici che si riscontrano durante i combattimenti dove si potranno effettuare degli attacchi simultanei (che non portano al consumo di punti speciali) e lo sblocco degli episodi extra posti dopo la storia principale.

In ogni scontro saranno presenti un massimo di sei mostri digitali, tre al massimo per ogni fazione. Il giocatore controlla di default il Digimon del leader e può impartire gli ordini anche ai due alleati modificando le impostazioni nel menu di strategia, altrimenti gli altri verranno controllati automaticamente dal computer. Il sistema utilizzato è quello dei combattimenti a turni, dove ogni creatura può utilizzare attacchi normali, abilità, fare uso di oggetti raccolti nei vari livelli, difendersi dai nemici oppure fuggire dagli scontri con i nemici selvatici.

Una volta terminato uno degli episodi principali (ad esempio l'episodio 2 per sbloccare Greymon, livello Campione di Agumon), un Digimon guadagna la possibilità di digievolvere in battaglia nella forma a livello Campione, Evoluto o Mega, raggiunto uno stadio successivo aumenteranno anche le statistiche del personaggio. Tuttavia ogni evoluzione costa dei punti tecnica (abbreviati in PT), come avviene per le abilità, ma a differenza di quest'ultime non fanno passare il proprio turno ad un altro membro della squadra o un nemico. Al termine di ogni battaglia, il Digimon regredirà automaticamente al livello Intermedio (tranne per Gatomon che è di livello Campione). In alcuni eventi (come ad esempio quando un mostro raggiunge la sua forma successiva per la prima volta), si presenterà nel livello già in quello stadio; in modo alternativo se si equipaggerà al Digimon la Digitessera "Promotore I", "Promotore II" o "Promotore III" potrà iniziare un incontro corrispettivamente al livello Campione, Evoluto e Mega.

Ogni sequenza di Digievoluzione presente nell'anime è stata completamente rianimata utilizzando la grafica del videogioco, così come per tutti gli altri filmati, eccezione fatta per la sigla iniziale, la cui unica differenza è il ridimensionamento in 16:9 per coprire in modo corretto lo schermo della console. Ogni sequenza video viene mostrata solamente la prima volta (tranne in alcuni casi in cui verranno riutilizzate nel corso della storia) ma potranno essere riviste nella Biblioteca, anche essa presente nel menu di pausa. Inoltre sono presenti anche alcuni brani musicali tratti dalla serie, Butter-Fly cantato da Kōji Wada e Brave Heart di Ayumi Miyazaki; il resto della musica si basa su melodie simili a quelle della serie animata assieme ad altre nuove.

In modo simile al sistema di equipaggiamento di altri videogiochi di ruolo come ad esempio la serie di Final Fantasy, il giocatore può equipaggiare delle Digitessere trovate nelle zone esplorate, le quali aumentano le statistiche (attacco, difesa, punti vitali, punti per le abilità e velocità) oppure consentono anche dei bonus ed abilità aggiuntive, come "Concentrazione" che aumenta di due stadi l'attacco e la difesa per alcuni turni, "Smezza PT" che dimezza il consumo dei PT, "Cura" per curare se stessi o un alleato ferito, "Digivita" che rianima un Digimon sconfitto una sola volta ed "Imboscata" che aumenta la possibilità di effettuare il primo colpo.

Le Digitessere sono suddivise per colore a seconda della categoria: potenziatori (arancione), comandi (blu), auto (verdi) e bonus (rosa).

In parallelo agli episodi basati sull'anime, ne sono presenti anche alcuni secondari che mostrano eventi inediti e non canonici con la trama originale, ma che servono per far aumentare il livello di Affinità dei ragazzi e l'esperienza dei propri Digimon. Inoltre vi è la possibilità di attraversare anche i Dedali Digitali, i quali sono dei Dungeon contenenti un maggior numero di avversari e di boss incontrati in precedenza.

Cambiamenti nella trama
Anche se la trama principale dell'anime non ha subito grandi cambiamenti, vi sono diverse scene in cui il gioco cambierà a seconda della decisione del giocatore oppure del suo livello di relazione.

 Episodio 3: Seadramon non viene svegliato da Tai ed Agumon che gli bruciano involontariamente la coda, ma viene pestato da T.K. quando questi si alza durante la notte.
 Episodio 5: Izzy può decidere se andare con il gruppo originale composto da Mimi, T.K. e Matt oppure con Sora e Joe. Il dialogo tra i personaggi cambierà a seconda della scelta, così come la presenza di Tai in uno dei due team.
 Episodio 7: Joe può scegliere se dar ragione a Tai oppure a Matt durante il loro litigio. In seguito Sora verrà con uno dei due ragazzi per aiutarlo contro Unimon a seconda della sua decisione.
 Episodio 13: Devimon, siccome è un boss molto potente, viene affrontato da Angemon e da altri due Digimon del party.
 Episodio 20: Etemon viene combattuto da MetalGreymon e da altri due Digimon presenti nel party per via della difficoltà della battaglia.
 Episodio 31: Oltre a Tai, Kari ed Izzy appaiono anche gli altri Digiprescelti ed ognuno di loro ha una missione da completare.
 Episodio 32: Biyomon e Palmon vincono la battaglia che ha come avversario SkullMeramon, mentre nell'anime le due non sono riuscite a tenergli testa ed è dovuto intervenire Greymon superdigievoluto in MetalGreymon per annientarlo.
 Episodio 33: Gabumon e Patamon vengono sfidati da Pumpkinmon e Gotsumon, evento che non avviene nella serie animata, in quanto i due non sono realmente intenzionati a far del male ai due Digimon ed ai loro partner umani. In seguito viene saltato lo scontro tra WereGarurumon, Angemon e Myotismon, difatti Patamon è l'unico a digievolversi ma poco dopo il Digimon malvagio si ritira momentaneamente.
 Episodio 37: Dopo che Gatomon è superdigievoluta in Angewomon, quest'ultima si scontrerà contro Myotismon assieme ad altri due compagni di squadra, questo cambiamento è stato apportato per rendere più semplice lo scontro.
 Episodio 39: WarGreymon e MetalGarurumon sfidano VenomMyotismon accompagnati da un terzo membro presente nella squadra. Questa modifica è stata apportata per permettere un ulteriore supporto al giocatore.
 Episodio 41: Joe può decidere se fermare il gruppo per farlo riflettere se il chiosco sulla spiaggia sia una trappola oppure no. Se Joe ferma il gruppo, Palmon non sarà costretta a combattere contro Scorpiomon ed in più il Digimon malvagio si potrà affrontare con altri due compagni.
 Episodio 42: WarGreymon non si scontrerà da solo con MetalSeadramon, infatti verrà aiutato da altri due compagni Digimon. Questo cambiamento è stato apportato probabilmente per rendere la battaglia più semplice al giocatore. Inoltre la scena in cui Whamon si sacrifica per distrarre MetalSeadramon è collocata prima dello scontro, al contrario dell'anime, dove avveniva durante lo stesso per salvare la vita a WarGreymon.
 Episodio 44: Gabumon sfida Cherrymon, anche se nella versione originale il Digimon di livello Evoluto si limita solamente a parlare con Matt.
 Episodio 47: Nella battaglia contro MetalEtemon, saranno presenti SaberLeomon ed Ogremon che forniranno supporto a Zudomon. Come negli altri casi dei boss, questo cambiamento è stato apportato per semplificare il gioco.
 Episodio 49: WarGreymon combatterà contro Machinedramon grazie all'aiuto di altri due membri della squadra, anche in questo caso perché la battaglia contro il nemico in questione risulta difficile.
 Episodio 51: Quando Joe e Gomamon trovano Matt e Gabumon vengono attaccati da un Vilemon, anche se nella versione originale questo Digimon non è mai apparso prima dell'incontro finale contro Piedmon.
 Episodio 52: Dopo che Piedmon ha sconfitto Tai ed il suo Digimon, sopraggiungeranno Matt e Garurumon per aiutare i loro amici, tuttavia WarGreymon regredirà allo stadio Intermedio tornando Agumon, anche se nei dialoghi successivi gli altri personaggi continueranno a riferirsi a lui come se fosse ancora al livello Mega. In seguito Gatomon non verrà catturata da Piedmon e poco dopo superdigievolverà in Angewomon per aiutare MagnaAngemon.
 Episodio 53: Dopo che i ragazzi sono stati cancellati da Apokarimon, questi riporta in vita alcuni dei loro peggiori nemici per farglieli sfidare. Se il giocatore avrà almeno 35 punti Affinità per ogni personaggio, potrà sbloccare la corrispettiva forma di livello Mega per i Digimon che non l'hanno mai ottenuta nella prima serie.
 Episodio 54: In seguito al ritorno dei digiprescelti nel loro mondo, si assisterà ad alcuni dialoghi aggiuntivi non presenti nell'anime.

Digimon presenti nel gioco

Digimon controllabili

Digimon di supporto
Nel corso della storia saranno presenti alcuni Digimon che si uniranno per brevi periodi di tempo alla squadra fornendo supporto al giocatore durante le battaglie come personaggi non giocanti. Per tutta la durata della loro presenza non possono essere rimossi dal party e vengono controllati solamente dal computer, fatta eccezione di Gatomon che diverrà giocabile alla fine dell'arco narrativo di Myotismon ed Omnimon nell'adattamento di Our War Game!.

Digimon non controllabili

 Primo stadio
 Botamon
 Punimon
 Yuramon
 Pagumon
 Poyomon
 Kuramon
 Tsumemon

 Intermedio
 Elecmon
 Gazimon
 DemiDevimon
 Otamamon
 Gizamon
 Gotsumon
 Mushroomon
 Floramon
 Betamon
 Keramon
 Veemon
 Guilmon
 Agumon (Savers)
 Hackmon

 Campione
 Kuwagamon
 Shellmon
 Monochromon
 Seadramon
 Numemon
 Capo dei Numemon
 Unimon
 Meramon
 Frigimon
 Mojyamon
 Sukamon & Chuumon
 Centarumon
 Leomon
 Ogremon
 Bakemon
 Lord Bakemon
 Whamon
 Drimogemon
 Kokatorimon
 Tyrannomon
 Vegiemon
 Nanimon
 Gekomon
 Devidramon
 Flymon
 Gesomon
 Raremon
 DarkTyrannomon
 Dokugumon
 Wizardmon
 Snimon
 Tuskmon
 Kiwimon
 Guardromon
 Mekanorimon
 RedVegiemon
 Tankmon
 Vilemon
 Chrysalimon
 Devimon

 Evoluto
 Monzaemon
 Andromon
 SkullGreymon
 Piximon
 Digitamamon
 Datamon
 Vademon
 ShogunGekomon
 Phantomon
 SkullMeramon
 Mammothmon
 Pumpkinmon
 MegaSeadramon
 Scorpiomon
 Divermon
 Blossomon
 Deramon
 Cherrymon
 Garbagemon
 Megadramon
 Gigadramon
 WaruMonzaemon
 LadyDevimon
 Parrotmon
 Etemon
 ChaosEtemon
 Myotismon
 Infermon

 Mega
 SaberLeomon
 MetalEtemon
 VenomMyotismon
 MetalSeadramon
 Machinedramon
 Puppetmon
 Piedmon
 Apokarimon
 Diaboromon
 Gallantmon
 ShineGreymon
 Gankoomon

 Armor
 Magnamon

 Spirit
 Agunimon
 KaiserGreymon

 Nessuno
 Shoutmon
 OmegaShoutmon
 Arresterdramon

Sviluppo
Digimon Adventure fu annunciato nel numero d'agosto 2012 della rivista nipponica V Jump come parte del quindicesimo anniversario del franchise e sarebbe stato progettato come una ricreazione della prima serie anime in modo completo su PlayStation Portable. Lo sviluppatore del gioco, Yūji Naka, ha annunciato tramite Twitter che il suo studio, Prope, avrebbe sviluppato il titolo come loro primo videogioco di ruolo. Un trailer fu pubblicato nel mese di settembre, dove venne rivelata la presenza dei doppiatori originali della controparte animata che avrebbero ripreso i loro corrispettivi ruoli per un totale di 70 ore di audio vocale. In aggiunta oltre alla serie, gli sviluppatori hanno incluso anche un livello basato sul film del 2000, Our War Game! assieme ad alcuni episodi secondari come bonus, che mostrano vicende mai narrate nella serie regolare.

Le prime copie del gioco vennero distribuite con un codice di produzione per PlayStation Portable per scaricare Digivice Ver. Portable, una versione emulata del Digimon virtual pet ed un buono acquisto che poteva essere riscattato per le carte da gioco presenti nel gioco per smartphone sviluppato da GREE, Digimon Collectors.

Accoglienza
Digimon Adventure ha venduto 47,807 copie nella settimana d'uscita, diventando il terzo videogioco più venduto di quel periodo nel Media Create software charts. Il titolo ha venduto un totale di 70,172 copie in Giappone prima di scendere dalla classifica arrivando il mese successivo al 30º posto tra i giochi più venduti. La rivista settimanale Famitsū gli ha dato un punteggio di 29 su 40 in base a quattro recensioni individuali dove ha ottenuto rispettivamente 8, 7, 7 e 7. Raffaele Staccini di Multiplayer.it classificò Digimon Adventure come l'ottavo miglior gioco della serie.

Note
Annotazioni

Fonti

Collegamenti esterni

Videogiochi di Digimon

redpajama_set_name: RedPajamaWikipedia


Online Consumer Mediation Centre (OCMC), National Law School of India University (NLSIU), Bengaluru, was inaugurated on the National Consumer Rights Day on 24th December, 2016 by Shri Ram Vilas Paswan, Hon'ble Minister, Consumer Affairs, Food and Public Distribution, Government of India Shri C.R. Chaudhary, Hon'ble Minister of State for Consumer Affairs, Food And Public Distribution, Government of India, Shri Hem Pande, Secretary, Department of Consumer Affairs, Ministry of Consumer Affairs, Food & Public Distribution Government of India (GoI) and Hon'ble Justice Shri D.K. Jain, President, National Consumers Disputes Redressal Commission (NCDRC) at Vigyan Bhavan, New Delhi.
Understanding the need for non-adversarial conflict resolution in consumer disputes, the Chair on Consumer Law and Practice at National Law School of India University had for the first time in India, disembarked on a mission of setting up an Online Consumer Mediation Centre. The initiative has been whole-heartedly supported by the Ministry of Consumer Affairs, Government of India, both in words and action. The Mediation Centre has developed an online platform with motto 'Anytime Anywhere Dispute Resolution' that ensures confidentiality and privacy at every stage of the online mediation. A dedicated website is designed to provide a user-friendly, transparent and secure online mediation process. An advisory committee is set up at the mediation centre to assist the Centre at every stage of development and appointment of expert mediators to the panel, from among those with professional and technical experience in different fields. The Centre has been advocating for quick and amicable settlement for both the consumers and businesses to preserve the relationship and trust between them which is the main agenda of the Centre. As a pilot programme, the Centre is confined to mediation services for consumer disputes in e-commerce only. The Centre runs with the vision to provide for an innovative online mediation tool that affords consumers better access to justice through quick and easy redressal mechanism and at the same time provide opportunity for businesses to maintain good customer relations. The mission of the Centre is to provide innovative technology for consumers and organisations to manage and resolve conflicts and to propel online mediation as a first choice to resolving consumer disputes. The values include Easy accessibility, Security, Confidentiality, Cost-effective, Neutrality and Integrity.


text:
package com.hkm.vdlsdk.realm;

import android.content.Context;

import io.realm.RealmConfiguration;

/**
 * Created by hesk on 21/12/15.
 */
public class RealmUtil {

    public static RealmConfiguration realmCfg(Context app) {
        return new RealmConfiguration.Builder(app)
                .deleteRealmIfMigrationNeeded()
                .build();
    }
}

redpajama_set_name: RedPajamaGithub


Symrise and FoodNavigator-USA held their annual VIP customer event in Chicago at the House of Blues on July 14th, 2013. We celebrated from 8PM to 1AM with hors d'oeuvres, an open bar and an evening filled with networking, entertainment, dancing and fun!
Tyler Bryant & The Shakedown hit the stage live to bring the night alive.
Symrise debuted the VodkaLand 2013 contest where the latest vodka flavor trends were revealed as six contestant finalists mixed live on stage before a panel of esteemed industry expert judges from Chilled Magazine and world renowned spirits companies.


Work, Employment, Skills and Training: Where Next for Scotland?
Labour market issues have been given very little attention in the independence debate. So today's launch of an ESRC funded research report on 'Work, Employment, Skills and Training: Where Next for Scotland?' is very welcome.
I was interviewed along with 67 other stakeholders as part of the research, so I was particularly interested in the report's findings. The complexity of the issue is illustrated by the multi-level governance with the EU, UK and Scottish Government all having a role, or in some cases shared responsibility. Given the shocking levels of productivity in the UK, it is surprising that skills utilisation in particular has not been given more attention.
Education, training and skills is probably the field least impacted by independence, because most is already devolved and Scotland has a very different system from the rest of the UK and England in particular. Professor Ewart Keep highlighted the structural focus on youth unemployment in Scotland, while in England there is little more than hand wringing. Advice and guidance services have collapsed in England, although I would argue they have been devalued in Scotland with too greater reliance on web based services. College regionalisation has come with significant cuts and it is too soon to judge its efficacy. The research also showed something of a disconnect on workforce development, particularly in 'unsexy' sectors like retail and social care. What the Scottish approach does provide is an ability to think collectively, rather than everything being left to the vagaries of the market.
Welfare to work and employability has similar challenges to the rest of the UK, with the concentration of disadvantage in geographical areas and amongst young people. While there was some support for the principles of welfare reform, the impact was actually adding to the barriers to getting people into work – not just getting them off benefits. The pressure is simply handed down to local services. There was a clear consensus in Scotland that there are problems at the bottom end of the labour market that will not be solved with benefit sanctions.
The research highlighted the importance of linking employability and health, strengthening employer engagement and more evidence of what works. There is a need to join up fragmented UK and Scottish provision and labour markets – a strong argument in my view for devolving many of these services. Not just to Holyrood, but also down to local level – recognising the risk of fragmentation of service and the loss of economy of scale. There is also a debate about how to incentivise employers either through the tax system or regulation.
On employment and the workplace, the report sets out the challenges including low pay, gender segregation and economic growth. The strength of the report is the focus on creating good jobs through job quality and design – with an understanding that employees are a source of innovation. There may be less clarity about how to make this happen, but options include using government as an exemplar and the use of procurement.
There is limited capacity in HR and organisational development and a less than cohesive employer voice, essential if the proposed social partnership model is to work effectively. Employer concerns about greater regulation and partnership in the research were more pragmatic than ideological. However, the White Paper model also requires a different model of capitalism in Scotland and there is little indication that the Scottish Government is ready for that radical journey. While there may be insufficient action on these issues in Scotland, none of this has even reached the UK government agenda! The research found that debates on the workforce in Scotland occupy a very different ideological space.
One conclusion is that whatever the outcome of the vote, much of the Scottish direction of travel is already fixed and unlikely to change. As the report says, "the new model is now on the table", even if the detailed road map is missing. The Mather Commission may fill in some of the gaps. It therefore remains open to debate if the proposals in the White Paper or greater devolution will remove the remaining barriers to progressive change.


text:
Q: AttributeError: 'NoneType' object has no attribute 'values' aiogram,sqlite3 выдаёт ошибку AttributeError: 'NoneType' object has no attribute 'values'
вот код:
@dp.message_handler(commands= ['sleep'])
async def sleep (message= types.Message):
   button1 = InlineKeyboardButton('Спать в центре', callback_data = '1')
   button2 = InlineKeyboardButton('Спать на краю', callback_data = '2')
   buttons = InlineKeyboardMarkup().add(button1, button2)
   await bot.send_message(message.chat.id, "Хорошо, вебери где хочешь спать: \n \nСпать в центре кровати: безопасно, но даёт меньше здоровья и денег, чем на краю. \nСпать на краю кровати: даёт много здоровья и денег, но есть шанс попастся серенькому волчку. \n \nЕсли вы попадётесь серенькому волчку, то у вас уменьшится здоровье, и волчок украдёт немного денег. ", reply_markup= buttons)

@dp.callback_query_handler(lambda c: c.data == '2')
async def process_callback_yes(callback: types.CallbackQuery, message= types.Message):
   rand = random.choice(["придёт", "не придёт"])

   await bot.delete_message(callback.message.chat.id, callback.message.message_id)
   await callback.message.answer("Вы легли спать на боку... Желаю удачи! ")
   await asyncio.sleep(120)
   if rand == "придёт":
       await bot.send_message(message.chat.id, f"О НЕТ! {user_name} УКУСИЛ ВОЛЧОК! \n-30 здоровья \n-10 денег \nДля лечения купи 'антикусь гель' в магазине: /shop")
       cursor.execute('UPDETE users SET hp= hp-30, SET money= money-10')
       db.commit()
   else:
       await bot.send_message(message.chat.id, f"Фухххххх. {user_name} смог спокойно поспать на боку! \n+60 здоровья \n+50 денег")
       cursor.execute('UPDATE users SET hp= hp+60, SET money= money=50')
       db.commit()

весь лог:
Task exception was never retrieved
future: <Task finished name='Task-22' coro=<Dispatcher._process_polling_updates() done, defined at C:\Users\Magicscreen\AppData\Roaming\Python\Python310\site-packages\aiogram\dispatcher\dispatcher.py:407> exception=AttributeError("'NoneType' object has no attribute 'values'")>
Traceback (most recent call last):
  File "C:\Users\Magicscreen\AppData\Roaming\Python\Python310\site-packages\aiogram\dispatcher\dispatcher.py", line 415, in _process_polling_updates
    for responses in itertools.chain.from_iterable(await self.process_updates(updates, fast)):
  File "C:\Users\Magicscreen\AppData\Roaming\Python\Python310\site-packages\aiogram\dispatcher\dispatcher.py", line 235, in process_updates
    return await asyncio.gather(*tasks)
  File "C:\Users\Magicscreen\AppData\Roaming\Python\Python310\site-packages\aiogram\dispatcher\handler.py", line 116, in notify
    response = await handler_obj.handler(*args, **partial_data)
  File "C:\Users\Magicscreen\AppData\Roaming\Python\Python310\site-packages\aiogram\dispatcher\dispatcher.py", line 283, in process_update
    return await self.callback_query_handlers.notify(update.callback_query)
  File "C:\Users\Magicscreen\AppData\Roaming\Python\Python310\site-packages\aiogram\dispatcher\handler.py", line 116, in notify
    response = await handler_obj.handler(*args, **partial_data)
  File "C:\Users\Magicscreen\Desktop\серенький волчок бот\bot.py", line 72, in process_callback_yes
    await bot.send_message(message.chat.id, f"О НЕТ! {user_name} УКУСИЛ ВОЛЧОК! \n-30 здоровья \n-10 денег \nДля лечения купи 'антикусь гель' в магазине: /shop")
  File "C:\Users\Magicscreen\AppData\Roaming\Python\Python310\site-packages\aiogram\types\fields.py", line 69, in __get__
    return self.get_value(instance)
  File "C:\Users\Magicscreen\AppData\Roaming\Python\Python310\site-packages\aiogram\types\fields.py", line 46, in get_value
    return instance.values.get(self.alias, self.default)
AttributeError: 'NoneType' object has no attribute 'values'

A: В функции async def process_callback_yes(...)
удалите message - его там нет
async def process_callback_yes(callback: types.CallbackQuery)

и обрашайтесь в этой функции так:
await bot.send_message(callback.message.chat.id,...)

redpajama_set_name: RedPajamaStackExchange


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This 2 wire pull chain light switch is UL recognized and CSA certified, therefore, it is safe to be used in any household application in USA and Canada. It is also universal and works with many ceiling fan manufacturers such as Hunter, Hampton Bay, Harbor Breeze, Westinghouse, Kichler, Casablanca, and others.
KTE 303A, Zing Ear ZE-119.


text:
Drugs are Bad, Mmkay? – Beautiful Boy
Bill	Reviews	 January 20, 2019 3 Minutes
With Oscar nominations coming up on Tuesday, there are two more films from 2018 that I want to see and review during the holiday weekend. It's very possible that with these two in the books, I might be so far ahead of the curve that I'll only have the Short categories to tackle for this year's Blitz.
Bearing that in mind, I finally got a chance to see Beautiful Boy a few days ago, thanks to my roommate's Amazon Prime account. I had wanted to see it during its theatrical run in the fall, but sadly it didn't succeed at the box office, earning only $10 million against its $25 million budget, making it a flop.
It's a shame, because the film has garnered widespread praise. This is the first English-language film from Felix Van Groeningen, previously nominated in the Foreign Language category for The Broken Circle Breakdown, and the lead performances from Steve Carell and Timothée Chalamet have been particularly noteworthy. Chalamet specifically has gotten significant buzz, garnering Supporting Actor nominations from the Golden Globes, BAFTA, and SAG. He'll almost certainly hear his name called on Tuesday morning as well, his second Oscar nomination in as many years. Between him and Lucas Hedges, the new generation of leading men is promising indeed.
The film is adapted from dual memoirs from the father-son pair of the film, David and Nic Sheff. Throughout the course of the film, Carell as David deals with Chalamet as Nic, while the younger suffers through bout after bout of drug addiction, rehab, and relapse.
Given that he's very likely to be nominated, the only real question to ask is, does Chalamet deserve his presumptive nomination? I can say that after watching the film, the answer is an unqualified yes. Chalamet gives the most dynamic performance of his young career, and the best portrayal of addiction for 2018. Mind you, this would be an improvement over Chalamet's last nominated performance simply by virtue of him not fucking a peach.
As Nic Sheff, Chalamet embodies addictive personality perfectly. The highs, the lows, the shame, the defiance, the desperation, the remorse, Chalamet covers so much ground he might as well be a tarp. This film was an ideal opportunity for the young star to flex his acting chops and display tremendous range. As such, he lifts up his co-star allowing Carell to deliver an equally compelling performance as a loving foil who increasingly runs out of options to help his oldest son while protecting his younger children from the reality of Nic's situation.
Chalamet's performance is even more impressive considering the number of addiction stories that have come out this year. Look at what we've had to this point: Don't Worry, He Won't Get Far on Foot, A Star is Born, Steve Carell's turn in Welcome to Marwen (which combined with the documentary Marwencol makes me want to retroactively lower its grade), and even as a secondary plot thread in Cold War, Bad Times at the El Royale, and Bohemian Rhapsody.
Nic's addiction issues are much more graphic and visceral than they are in other films. Bradley Cooper pisses himself at a fake Grammy ceremony, Timothée Chalamet snorts, shoots, cooks, smokes, swallows and does just about everything else drug-related you can imagine, to the point that Carell, playing Nic's father, actually snorts some himself just to try to understand the mindset his son keeps falling back on.
The film does get a bit maudlin, even to the point of mawkishness, but never did I feel like I was watching an Afterschool Special or some thinly-veiled Christian moralizing, like, say, Flight a few years ago. There's an honesty about Nic's predicament, an earnestness about wanting to change combined with helplessness in the face of the challenge. It's just a shame that the only likely nomination will be for Supporting Actor, while the guy who pissed himself will inexplicably get nominated for Best Actor, Director, and Picture come Tuesday.
Grade: A-
Join the conversation in the comments below! What film should I review next? How do you feel about addiction stories? Can we get rid of the accent above the "e" in Chalamet's name? It's really getting annoying having to pull up the special character menu! Let me know!
Felix Van Groeningen
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ISRAEL – Ramat Beit Shemesh - Remains of a unnamed Jewish town from the Second Temple period were found at the site, which boasts a large and rare collection of eight mikves (ritual baths), as well as wells, stone apparatus used for manufacturing products, and underground tunnels. According to project managers Sara Hirschberg, Sara Levavi-Eilat, and Shua Kislevitz, "What's special about this town is the vast scope of its private mikves, which were built into private homes. Every home here had a mikve and a well. Some of the ones we've uncovered are simple, and some are much more complex and include an "otzar" into which rainwater fell. "It's interesting to see how the residents were so stringent about the laws of purity. "Underneath the residential homes and stone manufacturing apparatus, we've found another surprising discovery from the Bark Kokhba revolt, which took place in the second century CE: a series of twisted escape tunnels which connected to complex underground systems. One of the tunnels accessed an underground well, to provide water for those in hiding. "In a cave, we found ceramic pitchers and whole cooking pots, which survived the rebels. These findings prove that people were still living in the area after Jerusalem's destruction in the year 70 BCE."
INDE – Ippagudem - Much to the delight of archaeologists and historians, a rare idol of Tara – the female Bodhisattva in Mahayana Buddhism who appears as a female Buddha in Vajrayana Buddhism – was found at Ippagudem in Station Ghanpur mandal recently. Archaeology and history enthusiast R Rathnakar Reddy found the black granite idol abandoned near the bund of a tank. He first mistook it for Yakshini of Jain mythology. But later, noted archaeologist and historian Emani Shivanagi Reddy confirmed it as Tara. "It was Shivanagi Reddy who identified the idol as Tara. There is an engraved image of Buddha on the hair bun. The deity's upper body is naked with large breasts, which is the most common description of Tara in Buddhist literature," Rathnakar said. Rathnakar also found a broken idol of Buddha near the black granite structure, which helped them confirm that it was Tara. Both the idols – three-ft-tall Tara and four-ft-tall Buddha – take historians and archeologists closer to the Buddhist era. It is believed that idol of Tara, which was damaged, belonged to 8th or 9th century AD.
FRANCE – Aix en Provence - Après un diagnostic réalisé par l'Inrap, qui a conclu à la présence d'une nécropole antique, la société privée Mosaïques archéologie a été retenue pour mener les fouilles préventives. Depuis le 13 février et jusqu'au 21 avril, une équipe d'archéologues auscultent donc deux zones définies, l'une de 3600 m² et l'autre, assez vaste, de près de 2 hectares qui semble être la plus riche en enseignements. "Nous avons là une nécropole qui s'étend sur environ 50 m de long et 25 m de large, située au nord d'un chemin empierré. À ce stade des fouilles, nous avons identifié entre trente et quarante fosses bûchers aux parois rubéfiées, dans un état de conservation au-delà de nos espérances", explique Olivier Mignot, responsable des opérations et spécialiste de l'Antiquité. Si les premières fosses n'ont livré que peu de vestiges, la dernière, fouillée ces jours-ci, a permis de mettre au jour de la vaisselle antique (des bols, une cruche, une lampe à huile) mais aussi et surtout... des ossements. Ce qui semble donc confirmer la destination funéraire du lieu. Ce qui soulève dans le même temps bon nombre de questions. Pourquoi les fosses sont-elles vides ? Y a-t-il eu nettoyage et ponction des ossements ? Pour les placer où ? Et à quelle période est-ce intervenu par rapport à la crémation ? Autant d'interrogations qui trouveront peut-être une explication à l'issue des fouilles, lorsque l'ensemble des données recueillies sur le terrain par les archéologues seront analysées en laboratoire. Des vases funéraires ont également été identifiés. Reste à savoir ce qu'ils contiennent. Autre découverte, celle d'une construction en pierre. "Peut-être un mausolée", avance Olivier Mignot qui espère, en creusant plus profondément, trouver "des preuves. Des vases ossuaires, ce serait l'idéal." Tout l'enjeu étant, au fond, de comprendre les rites funéraires de cette époque, datée au plus tard du IIIe siècle après JC. Une "période charnière entre les rites romains et chrétiens." Des suppositions qui devront être confirmées en phase "post-fouilles".
ARMENIE - Chouchi - Armenia has begun excavations at Govhar Agha Mosque, referred to as Persian Upper Mosque by Armenians, in the occupied Azerbaijani city of Shusha, APAreported citing Armenpress. The excavation work is being carried out by the Revival of eastern historic legacy foundation. The mosque was built in 1768 upon the order of Ibrahim Khan of Garabagh. However, the construction came to a halt afterwards but was completed in 1883 with the aid of Karbalai Safi Khan Garabaghi.
INDE – Odisha - A civilisation of the Stone Age has been discovered during a research by the Archaeological Survey of India in Chandaka Sanctuary on the outskirts of Odisha's capital. A team led by ASI's Bhubaneswar circle deputy superintendent D.B. Garnaik revealed that there was human habitat in the hill caves located in the north-west of the forest, approximately 4,000 years ago. During a three-month-long research in the wildlife reserve, the team found ancient stone carvings. Primary statistics revealed that the artwork on reptiles, weapons and geometrical signs prove that people were living in Parthapur, Kusapangi and Gayalbank, 20 km away from Cuttack and 40 km from Bhubaneswar, at least 3,500-4,000 years ago. The artworks found from the site are assumed to be of the new Stone Age and Copper Age. The caves inside the hills have been named as Pandav Bakhara, Duara Khola, Tiger Cave, Chanchali Cave, Kalia Taila Cave, Narahari Cave and Anahat Cave. In these cases, artworks of the Copper Age and the Stone Age have been found. There is a lake adjacent to the hill near Mahanadi River. It is assumed that there was a civilisation near the river during that period.
CHYPRE – Limassol - Archaeological finds possibly dating from the 13th century have been discovered during roadworks in Limassol's old town, the antiquities department said on Monday. "Foundations of architectural remains of a monumental medieval building have been found on Ayias Theklis street," archaeological officer Giannis Violaris told the Cyprus Mail. "It didn't come as a surprise that we found these antiquities, it is an area rife with history as it is so close to the castle. We were prepared for this." Stratigraphy is the next step the antiquities department will take, trying to discover if there are older archaeological finds under the most recently discovered ones that could be from an older time. "The ones we have found are most likely from the Middle Ages. There could be something underneath that from earlier," Violaris said.


Fetna Mikati, a Kent State University professor in the Department of Modern and Classical Languages, does not believe in lecturing her students. Mikati believes in enriched discussions and using unconventional teaching tools to reach the goals set for them. And that is one of the reasons she was nominated and honored with an Outstanding Teaching Award.
The Outstanding Teaching Award is presented to full-time, non-tenure track or part-time faculty members who consistently show outstanding teaching skills in the classroom.
Jamil Kassabri, a junior criminology and justice studies major, enjoys playing the games that Mikati uses when teaching.
One of the most memorable teaching moments for Mikati is knowing that she is connecting with her students.
Her students are able to see how much she cares about them and they appreciate the unique teaching methods she uses.


Brain Res. 1990 Apr 23;514(1):131-4.
Excitatory amino acid antagonists protect mice against seizures induced by bicuculline.
Turski WA1, Urbanska E, Dziki M, Parada-Turska J, Ikonomidou C.
Department of Pharmacology, Medical School, Lublin, Poland.
The effects of excitatory amino acid antagonists on convulsions induced by intracerebroventricular (i.c.v.) or systemic (s.c.) administration of the gamma-aminobutyric acidA (GABAA) antagonist bicuculline (BIC) were tested in mice. 3-[+/-)-2-Carboxypiperazin-4-yl)-propyl-1-phosphonate (CPP), 2-amino-7-phosphonoheptanoate (AP7) and (+)-5-methyl-10,11-dihydro-5H-dibenzo(a,d)cycloheptan-5,10-imine maleate (MK-801) were used as representatives of N-methyl-D-aspartate (NMDA) antagonists. gamma-D-Glutamylaminomethylsulphonate (gamma-D-GAMS) typified a preferential kainate (KA) antagonist, 6-cyano-7-nitro-quinoxaline-2,3-dione (CNQX) represented a preferential quisqualate (QA) antagonist, and kynurenic acid (KYNA) was used as a mixed NMDA/KA antagonist. Bicuculline methiodide (BMI) induced clonic convulsions following i.c.v. administration with a CD50 of 0.183 nmol (range 0.164-0.204). The excitatory amino acid antagonists blocked clonic seizures induced by BMI in the dose of 0.224 nmol (approximately CD97) when coinjected into the lateral ventricle. CPP (ED50 0.0075 nmol) was the most potent anticonvulsant and was followed by AP7 (0.182 nmol), MK-801 (0.22 nmol), gamma-D-GAMS (0.4 nmol), KYNA (1.7 nmol) and CNQX (5.17 nmol). Muscimol (MSC), the GABAA agonist, blocked BMI-induced seizures with an ED50 of 0.25 nmol. Systemic (s.c.) administration of BIC induced in mice generalized seizures with a CD50 of 2.2 mg/kg (range 1.9-2.5) for clonus and CD50 of 2.4 mg/kg (range 2.2-2.7) for tonus.2+ the pathogenesis of seizures triggered by bicuculline in mice.