text:
\section{Introduction}
\label{intro}
Coherent scattering processes in the solar atmosphere causes the emitted radiation
to be linearly polarized. The spectrum so obtained is referred to as the
Second Solar Spectrum (SSS). This linearly polarized spectrum gets modified
at the line core in the presence of weak magnetic fields due to the Hanle effect. One
of the commonly observed and well studied lines in the SSS is the
strong, chromospheric Ca {\sc i} 4227 \AA{} line \citep[see for example,][]{stenetal80, sten82,
gandorfer2002}.
This is a normal Zeeman triplet line arising due to transition between
the atomic states with total angular momentum $J=0 \to 1 \to 0$. It
exhibits largest scattering polarization among all lines in the
Sun's visible spectrum \citep{stenetal80}.
The core of the Ca {\sc i} 4227 \AA{} line is formed around a height of about
1000 km above the photosphere making it chromospheric in nature.
The Hanle effect in the core of the Ca {\sc i} 4227 \AA{} line
was first observed by \citet{sten82}.

One of the interesting feature exhibited by this line is
the spatial variation of the wing polarization in $(Q/I, U/I)$ spectra along the
spectrograph slit. \citet{biandaetal03} noticed these variations
in the observations near an active region. Later these spatial
variations were also observed in quiet regions by
\citet{sampetal09} and were interpreted to be
arising due to the local inhomogeneities in the atmospheric layers. A detailed modeling of the
Ca {\sc i} 4227 \AA{} line profile observed in a quite region near the solar limb is presented
by \citet{lsa10}. The authors employed last scattering approximation to model them.
Observations of the forward scattering Hanle effect in the Ca {\sc i} 4227 \AA{} line near the disk
center were performed by \citet{bianda11}. Subsequently these observations were
modeled by \citet{FS11} to determine the chromospheric weak magnetic fields.

One of the early attempts to model the polarization profiles
of the Ca~{\sc i}~4227~\AA\ line
observed in both quiet and active regions was by \citet{mf92}.
The author used the observations of \citet{sten82}.
Her treatment included the effects of partial frequency redistribution (PRD)
and radiative transfer (RT).

To better understand the physics of scattering and to exploit
it for various diagnostic purposes,
we need to systematically study the center-to-limb variation (CLV) of the SSS.
This will help us sample the height information of the atmospheric parameters
and magnetic fields, as observations made at different lines of sight (LOS) sample different heights in the solar atmosphere.
Few attempts have been made so far in detailed modeling of the CLV observations of
($I$, $Q/I$) spectra of atomic and molecular lines in the SSS.
The most challenging aspect of such CLV modeling is to find a single model
atmosphere which can fit both $I$ and $Q/I$ at all limb distances $\mu~(=\cos \theta)$,
simultaneously. One such attempt was made by \citet{holandsten07}
to model CLV of the Ca {\sc ii} K line. They discuss the possibility of constructing a
two-component atmospheric model (using a combination of a hot and a cool atmospheric component) to
achieve a fit to the observed CLV profiles. A height dependent mixing ratio was
required by them in order to simultaneously fit $I$ and $Q/I$ spectra at all the limb distances.
They also demonstrate that a single atmospheric model with optimized temperature structure
can be used to achieve a fit to the Ca {\sc ii} K line CLV data.
However they find that different extents of modification in
the temperature structure are required for different limb distances ($\mu$).
Another paper in which such CLV studies
have been done is that of \citet{shapiro11} who consider the molecular CN violet system.
They discuss the general problems involved in obtaining a
simultaneous fit to the $I$ and $Q/I$ profiles using the standard
1-D single atmospheric model, as well as two-component atmospheric models.
They finally construct an anisotropy modified single 1-D
atmospheric model to simultaneously fit $I$ and $Q/I$ at all $\mu$.

The CLV of the Ca~{\sc i} 4227~\AA\ line away from the active regions was
first observed by \citet{stenetal80} and analyzed by \citet{aueretal80}.
The CLV of the line center polarization observed by \citet{stenetal80}
was later used by \citet{mf94} to study the Hanle effect
due to the magnetic field canopies in the chromosphere.
The CLV observations of this line was also done by \citet{bianda98,bianda99}.
In this paper we attempt a detailed simultaneous modeling of the observed CLV of both $I$
and $Q/I$ profiles of the Ca {\sc i} 4227 \AA{} line.
For this purpose we solve the polarized RT equation by taking account of
PRD effects in the non-magnetic regime. Standard 1-D atmospheric FAL models
\citep{font93, avrett95} are used to obtain a fit to the $(I, Q/I)$ spectra. We find that it is not
possible to achieve a simultaneous ($I, Q/I$) fit to the CLV observations with a single 1-D model atmosphere.
If we consider the CLV of $Q/I$ alone, then we find it necessary to modify the original
temperature structure of the standard FAL atmospheric models to obtain a fit.
Such modifications of the original temperature structure were also used in
previous works by \citet{holandsten07, smietal12, smietal13}. In the present paper, the original
temperature structure of the standard FAL-A atmosphere is modified. Later, the
modified FAL-A ($\overline{{\rm FALA}}$) is combined with FAL-X atmospheric
model to construct a single component model. It turns out that this newly constructed
combined model can closely reproduce the observed $Q/I$ at different limb distances.

In Section~{\ref{obsevations} we give the details of the CLV observations. Section~{\ref{modeling}}
is devoted to the modeling procedure and the results. Section~\ref{depth-dependence} describes the
observational analysis to determine the magnetic fields. Concluding
remarks are given in Section~{\ref{conclusion}}.

\section{Observational details}
\label{obsevations}
\begin{figure*}
\centering
\includegraphics[scale=0.6]{fig1.eps}
\caption{CCD images of $I$ (only for $\mu = 0.1$) and $Q/I$
at 5 selected $\mu$ values of the Ca {\sc i} 4227 \AA{} line.
The observations were taken on October 16, 2012 at IRSOL in Switzerland.}
\label{ccd}
\end{figure*}

The CLV observations of the Ca {\sc i} 4227 \AA{} line presented in this paper were
obtained with the Zurich Imaging Polarimeter-3 (ZIMPOL-3) \citep{ramellietal10}
at IRSOL (Istituto Ricerche Solari Locarno) in Switzerland on October 16, 2012.
The observations were taken at 14 different $\mu$ positions (0.10, 0.15, 0.20, 0.25, 0.30, 0.35,
0.40, 0.45, 0.50, 0.60, 0.70, 0.80, 0.90 and 1.0) starting from the
heliographic north pole at $\mu=0.1$ up to the disk center at $\mu=1$. Figure~\ref{ccd}
shows the CCD images of the Ca {\sc i} 4227 \AA{} line at 5 selected positions on
the solar disk. The polarization modulation was done with a piezo-elastic modulator
(PEM). The spectrograph slit was 60 $\mu$m wide corresponding to
a spatial extent of 0.5$\arcsec$ on the solar disk. The CCD covered
190$\arcsec$ along the slit. The CCD images have 140
effective pixel resolution elements in the spatial
direction, with each element corresponding to 1.38$\arcsec$, and
1240 pixels in the wavelength direction, with one pixel corresponding to 5.30 m\AA{}.

To keep the solar image position stable, the primary image guiding system is
used \citep{kulvere11}. In addition, below $\mu = 0.35$ a rotating
glass tiltplate is used to keep under control the distance between the
spectrograph slit and the solar limb image. The slit jaw image is digitized
by a dedicated CCD camera. An algorithm recognizes the solar limb and
the spectrograph slit position on the image. This allows the calculated desired distance between the
limb and the slit to be set by automatic control of the tilt plate. Note
that this plate is set after the polarization analyzer and hence does not
introduce spurious polarization signatures.
At each $\mu$ position a measurement is obtained by adding 300 single frames,
each of them are obtained with an exposure time of 1 sec.
Therefore the effective integration time is 8 minutes. The
precision of the pointing at a chosen $\mu$ position over 8 minutes using
the tiltplate is limited to about 1$\arcsec$, which is less than the size of one pixel.

An improvement of these measurements is related to the absolute precision
which we could reach in measuring $Q/I$. Previously, the zero polarization value
needed to be defined manually was based on indirect considerations (for example
the CLV of the continuum polarization). For the data set described in this
paper we could reach an absolute precision of about $5\times10^{-5}$.  This is
mainly due to: a) the precise control of limb distance, allowed by the
tiltplate system described above, b) the improved control of the rotation
of the optical devices, including the polarization analyzer in front of the
slit (to compensate for the image rotation originated by the Gregory Coud\`e
telescope), and c) the optical compensation of the instrumental linear
polarization, which is a source of variable offset effects, with an oriented glass
plate set in front of the polarization analyzer.
It was thus possible to subtract from every measurement done at a defined
$\mu$ position, the polarization level measured at disk center in a quiet
region. For symmetry reasons the linear polarization in the continuum
is expected to be zero at the disk center. In this way all residual instrumental linear
polarization signatures are taken into account.

\subsection{Stray light correction}
\label{stray-light}
The observed profiles contain contribution from the spectrograph stray light which is about 2 \% of the
continuum intensity. Here we correct both the intensity and polarization profiles for stray light.
The effect of stray light, including both its intensity and polarization, was treated in \citet{stenflo74}.
Below are the details of the procedure we have followed.

In the absence of stray light but with instrumental polarization (cross talk from $I(\lambda)$),
the $I(\lambda)$ and $Q(\lambda)$ parameters after polarization calibration are
$I'(\lambda)$ = $I(\lambda)$ and $Q'(\lambda)$ = $Q(\lambda) + M_{21}I(\lambda)$, if
we assume that the Mueller matrix has been normalized ($M_{11} = 1$), there is no telescope
depolarization or it has been calibrated away ($M_{22} = 1$), and that polarization cross talk
from $U$ and $V$ can be disregarded. $M_{21}$ is the spectrally flat instrumental polarization,
which for convenience will be renamed as $p_z$, since it represents a flat offset of the zero point
of the polarization scale.

In the presence of stray light with an intensity that is a fraction $s$ of the continuum
intensity $I_c$ and has a polarization $p_s$, the apparent or observed Stokes parameters are
\begin{eqnarray}
 && \!\!\!\!\!\!\!\!\!\!\!I_{obs}(\lambda) = I(\lambda) + sI_c, \nonumber \\&&
\!\!\!\!\!\!\!\!\!\!\!Q_{obs}(\lambda) = Q(\lambda) + p_z (I(\lambda) + sI_c) + p_s sI_c.
\label{obsestokes}
\end{eqnarray}
We now introduce the notation $r(\lambda)$ = $I(\lambda)/I_c$ and
$r_{obs}(\lambda)$ = $I_{obs}(\lambda)/I_{obs,c}$ for the rest intensities.
For clarity we attach a
$\lambda$ to the quantities that are spectrally structured, in contrast to the three free parameters of
our problem, namely, $s$, $p_s$, and $p_z$, which are constant and spectrally flat. Then
\begin{equation}
r(\lambda) = (1 + s) r_{obs}(\lambda) - s.
\label{rlambda}
\end{equation}
Similarly we define the intrinsic polarization $p({\lambda}) = Q(\lambda)/I(\lambda)$
and the apparent polarization $p_{obs}(\lambda)$ = $Q_{obs}(\lambda)/I_{obs}(\lambda)$.
One can easily show that
\begin{equation}
 p({\lambda}) = \bigg(1 + \frac{s}{r(\lambda)}\bigg) [ p_{obs}(\lambda) - p_z ] -
\frac{s}{r(\lambda)} p_s.
\label{plambda}
\end{equation}
To calculate $p(\lambda)$ from the observations we need to insert the expression for $r(\lambda)$
from Equation~(\ref{rlambda}) into Equation~(\ref{plambda}).

$p_s$ represents the intrinsic polarization as averaged over the wide spectral range
that contributes to the stray light. A major source of spectrograph stray light are grating
ghosts that sample discrete wavelengths spread over a large wavelength range. In the
absence of other information, the best estimate of $p_s$ is probably $p_s \approx p_c$,
i.e., to set it equal to the continuum polarization.

The determination of $p_z$ is best made for a disk center recording that is done immediately
before or after the measurement at the given $\mu$ position (so that one can assume
that the instrumental polarization has not changed). At disk center the solar scattering
polarization is zero, so the apparent polarization that we see is simply $p_z$ (in contrast to
measurements of disk center, where $p_z$ is mixed with intrinsic solar polarization).

It is important to realize that the problem of correcting for the zero point of the
polarization scale is entirely decoupled from the stray light issue. It is the first step to be
done, and it gives us the spectrum
\begin{equation}
 p'(\lambda) = p_{obs}(\lambda) - p_z,
\label{pprimelam}
\end{equation}
which would equal to $p({\lambda})$ in the absence of stray light. To correct $p'(\lambda)$
for stray light we do not need to refer to $p_z$ or disk center observations.
The way in which the stray light correction enters can be seen by rewriting Equation~(\ref{plambda})
as
\begin{equation}
 p(\lambda) = p'(\lambda) + \frac{s}{r(\lambda)} (p'(\lambda) - p_s).
\label{plamnew}
\end{equation}
If the stray light were unpolarized, then the stray light scaling factor $s/{r(\lambda)}$,
which is large where the rest intensity $r(\lambda)$ is low, acts to amplify the polarization
amplitudes $p'(\lambda)$. In the presence of stray light polarization, however,
the scaling factor only acts on the amplitude
with respect to the $p_s$ level rather than with respect to the zero level.
The stray light polarization therefore reduces the effect of the stray light correction.
For polarization amplitudes that is equal to $p_s$ (which represents a broad band polarization
background that may be approximated with the continuum polarization level $p_c$), the
stray light correction does not have any effect at all. For the Ca {\sc i} 4227\AA{} line, however, the
core polarization is usually larger than $p_c$. In this particular case the stray light polarization
becomes a second-order effect (since $sp_c$ is a product of two small quantities).
Parameter $s$ is determined exclusively from fitting the Fourier Transform Spectrum (FTS)
of \citet{kurucz84}, in
the same context as the spectral broadening is determined.
The above considerations give us a rather well defined procedure to determine (within
the framework of our idealized model) unique estimates of the parameters $s$, $p_z$, and $p_s$.
Using these estimates we can correct both the $I(\lambda)$ and
$Q(\lambda)/I(\lambda)$ spectra
for stray light. In other sections we have dropped the $\lambda$ dependence
of $I$ and $Q$ for notational simplicity.

While the observed spectra are corrected for stray light, they have not been
corrected for spectral broadening, because the instrumental profile is not known with
the precision that is needed to allow a deconvolution.
The theoretical spectra on the other hand, which are used for comparison with the
observed spectra, need to be spectrally broadened to emulate the observations. However,
one should not apply stray light to the theoretical spectra, since one can easily do the
correction to the observed spectra itself. In this way we keep the presentation of the
theoretical results independent of the particular properties of the instrument used for the
observations, with the single exception of spectral broadening.

\begin{figure*}
\centering
\includegraphics[scale=0.7]{fig2.eps}
\caption{Temperature structure of four standard models FAL-A, FAL-C, FAL-F and FAL-X used in our
studies. Along with these standard models the temperature structure of the new model atmosphere
$\overline{{\rm FALA}} + {{\rm FALX}}$ is also shown.}
\label{temp-structure}
\end{figure*}

\begin{figure*}
\centering
\includegraphics[scale=0.5]{fig3.eps}
\caption{Observed (solid line) and calculated intensity and polarization signals as function
of $\mu$ (observed at 14 points) at three different wavelength positions in the line profile.
The spectra are calculated for standard models FAL-X, FAL-C, FAL-A, and FAL-F.}
\label{clv-plots}
\end{figure*}

\section{Modeling of the CLV observations}
\label{modeling}
In this section we describe the modeling procedure we have followed to model the
CLV of the Ca~{\sc i} 4227~\AA\ line. We started with an aim of finding a single 1-D atmosphere
that can simultaneously
fit ($I$, $Q/I$) CLV of the Ca~{\sc i} 4227~\AA\ line.
As a first step towards this, we
begin the modeling of the observed profiles by
solving the polarized RT equation for a two-level atom.
The one-dimensional polarized RT equation along with the other necessary equations,
in the non-magnetic regime, used in this paper are described
in detail elsewhere \citep[see][]{lsa10}. The elastic collision rates used in this paper
are computed following the theory presented in \citet{barklem97}.
Also, the modeling is done here using a two-stage process
where the intensities are computed using a PRD capable MALI
(Multi-level Approximate Lambda Iteration) code
of \citet{rh01} in the first stage. In the second stage,
the polarization profiles are computed perturbatively by solving the polarized transfer
equation. The details of such a two-stage
modeling procedure is described in \citet[][see also \citealt{lsa10}]{reneetal05}.
The atom model of the Ca~{\sc i} used in the present paper is same as the one
discussed in \citet{lsa10}. Hence we do not repeat the details here.

In our studies we use four standard 1-D model atmospheres of the Sun
namely - FAL-A, FAL-C, FAL-F \citep{font93} and FAL-X \citep{avrett95}. The temperature structure
of these models are shown in Figure ~\ref{temp-structure}. Along with the standard models, the
temperature structure of our newly constructed model $\overline{{\rm FALA}} + {{\rm FALX}}$ is
also shown in the figure, details of which will
be discussed in Section~\ref{newmodel}.

\subsection{CLV behavior at three wavelength positions}
The observed $Q/I$ profiles of the Ca~{\sc i}~4227~\AA\ line show
three prominent features. They are, the line center at 4226.7~\AA, the
blue wing PRD peak at 4226.2~\AA\ and the red wing PRD peak at 4227.1~\AA.
While the line center of the Ca {\sc i} 4227 \AA{} line is formed within a height range of
700 - 1000 km (covering $0.9 \leqslant \mu \leqslant 0.1$), the blue and the red wing PRD peaks are formed
at a height of 150-250 km above
the level where the vertical continuum optical depth at 5000 \AA{} is unity.
To get an idea of the behavior of the polarized spectra as a function of $\mu$, we plot
the angular dependence of intensity (only at line center) and linear polarization at these chosen
wavelength positions in Figure~\ref{clv-plots} computed using the standard 1-D model atmospheres.
As expected, it can be seen from Figure~\ref{clv-plots} that the
degree of linear polarization decreases to zero towards the disk
center due to symmetry in the scattering geometry.

Panels (a) and (b) of Figure~\ref{clv-plots} show a comparison of the observed and theoretical
CLV of $I$ and $Q/I$ respectively at the line center wavelength.
We see that the hottest model FAL-F (dot-dashed line) is more suited for modeling the CLV of
line center intensity.
But the same model is not at all good for $Q/I$. Instead it is the coolest model FAL-X which provides
the closest fit to the observed $Q/I$.
This contrasting behavior seems to point at the fact that we need two different temperatures
to simultaneously fit $I$ and $Q/I$ at the line center. From Figure~\ref{clv-plots} (b)
we see that the theoretical profile computed using FAL-A also falls close to the observed
CLV profile of $Q/I$.
We consider the FAL-X atmosphere rather than FAL-A to provide a better fit to the
observed $Q/I$ at the line center for the following reasons:
At the line center and when $\mu$ is small, we always expect the non-magnetic $Q/I$ amplitude to be
larger as compared with the observed $Q/I$, because the observed $Q/I$
includes depolarization by magnetic fields. As we go to larger $\mu$ the magnetic fields
may enhance the core polarization amplitude. Such a behavior was noted
by \citet{mf94}, who points out that there are enhancement effects due to
magnetic fields when $\mu > 0.4$ (this will be discussed in detail in Section~\ref{results}).
We found the FAL-X model to better satisfy this behavior.
Thus we see from Figure~\ref{clv-plots} (b) that the theoretical
values of $Q/I$ at line center when computed with FAL-X
are larger than the observed $Q/I$ for $\mu < 0.4$, while FAL-A shows this behavior
only for $\mu < 0.25$.
Besides this, the theoretical $Q/I$ computed with FAL-A falls much below the
observed $Q/I$ as we move towards
larger values of $\mu$.
For these reasons we consider FAL-X to give a consistent overall fit to the observed CLV
of $Q/I$ at line center, while FAL-A does not.

On the other hand, Figures~\ref{clv-plots} (c)
and (d) show the CLV profiles of $Q/I$ at the blue and red wing PRD peak wavelength positions
respectively. We notice that both FAL-F and FAL-X model atmospheres fail to provide a fit to the
PRD peaks. It is the theoretical CLV profiles from the FAL-A model that falls closest to the
observed CLV of $Q/I$.
Thus we do not find a single 1-D atmospheric model which can
provide a fit to the entire Stokes ($I$, $Q/I$) profiles simultaneously. As a next step we
explore the possibility of obtaining a fit to the CLV of the Stokes profiles through small
modification of the temperature structure at appropriate heights, of the original FAL models.

\subsection{Theoretical fit to the CLV of $Q/I$ profiles}
\label{newmodel}
From Figures~\ref{clv-plots} (c) and (d) we see that though the theoretical profiles from the
model FAL-A falls closest to the observed CLV of $Q/I$, it fails to provide a
satisfactory fit to the {$Q/I$ observations}. In order to obtain a better fit to the
observed CLV of $Q/I$ profiles, we adopt
modification of temperature structure
at the heights where PRD peaks are formed.
We focus our attention only on fit to the $Q/I$ profiles.
Since FAL-A model atmosphere provides closest fit
to the observed $Q/I$ profiles, we choose this model for further modifications.
Accordingly, the temperature of the FAL-A standard model at these heights is reduced by about 200 K.
This newly constructed model is denoted as $\overline{{\rm FALA}}$.
This new model provides a better fit to the wing PRD peaks at all the limb distances.

After achieving a fit to the PRD peaks, we concentrate on obtaining a fit to the
linear polarization at the line center. From Figure~\ref{clv-plots} (b) we see that it is the
FAL-X model atmosphere which fits the observed profiles, the closest. Thus,
to obtain a satisfactory fit to the entire $Q/I$ profile
we need to combine these two model atmospheres ($\overline{{\rm FALA}}$ and FAL-X) at appropriate
heights.
The two models are combined such that the new model atmosphere has the temperature structure of
$\overline{{\rm FALA}}$ up to a height of ~400 km, and the temperature structure
of FAL-X
in the heights above 400 km.
The temperature structure of the new combined model atmosphere
($\overline{{\rm FALA}} + {{\rm FALX}}$)
is shown as the solid line in Figure~\ref{temp-structure}.
The results obtained using this combined model atmosphere are discussed below.

\subsubsection{Results from the new combined model atmosphere}
\label{results}
The theoretical profiles obtained using $\overline{{\rm FALA}} + {{\rm FALX}}$ model atmosphere
are shown in Figure~\ref{profiles} (dotted line). Also a comparison between the observed and theoretical
$Q/I$ CLV curves at the blue and red wing PRD peaks and at the line center wavelength
using the combined model is shown in Figure~\ref{clv-new} (dotted line).
These theoretical profiles show that we obtain an overall satisfactory fit
to the $Q/I$ profiles at all the $\mu$ positions using the
combined model atmosphere. The theoretical profiles computed using the combined model atmosphere
in Figures~\ref{profiles} and \ref{clv-new} include suitable spectral smearing.
This is done by convolving the theoretical spectra with a Gaussian profile having a
FWHM of 50 m\AA{}.
The smearing accounts for both the instrumental broadening (40 m\AA{}) and
the broadening by macro-turbulent velocity fields (30 m\AA{}). The macro-turbulent
smearing corresponds to a velocity of 1.28 km/s. For the deep lines like the
Ca {\sc i} 4227 \AA{}, the effects of the stray light corrections (the
stray light correction procedure is described in
Section~\ref{stray-light}) are much more important than the smearing. The intensity ($I$)
profiles from the combined model seem to fit the observed data at all the $\mu$
positions, with the exception of the line core, where we fail to get a satisfactory fit. At the
formation heights of the line center, a rest intensity fit requires a
hotter atmospheric model like the FAL-F which
is not suitable for achieving a good fit to the
$Q/I$ profile - which indeed requires cooler models like the FAL-X.
In spite of the carefully determined stray light correction (by $s$ = 2\%) to the
observed Stokes $I$ profiles, the central line depth still does not come close to reproduce
the very deep theoretical $I$ profiles.
We have also carried out tests with the use of different micro- and macro-turbulent
velocities, and we found that the choice of turbulent velocity does not significantly
affect the rest intensity of the Stokes $I$ profiles.

From Figures~\ref{profiles} and \ref{clv-new} we notice that for $\mu \leqslant 0.35$
the observed line center $Q/I$ is less than the theoretical value and for
$\mu > 0.35$ it is greater than the $Q/I$ predicted theoretically.
Such a discrepancy was also encountered by \citet{mf94} while modeling the
CLV of the line center $Q/I$ of the Ca~{\sc i}~4227~\AA\ line.
The author found that the ratio of $(Q/I)_{\rm obs}$ and $(Q/I)_{\rm theory}$
at the line center was close to unity for smaller $\mu$ values ($\mu < 0.4$) and
much greater than one for larger $\mu$ values.
However her treatment did not include the stray light corrections.
We recall that the observed profiles in Figure~\ref{clv-new} are corrected for the
stray light.
In \citet{mf94} though an explanation of the physical mechanism behind this enhancement in
polarization for larger $\mu$ values was anticipated based on accelerated motions in the chromosphere,
but it was not completely justified.

To examine this discrepancy further, we plot the variation exhibited by
$Q/I$ along the spectrograph slit at the line center (solid line) and compare it with the $Q/I$
in the blue wings (dotted line) in Figure~\ref{slit-variation}. The observed
line center $Q/I$ values are smoothed over a rectangular box corresponding to
5$\arcsec$ to reduce contribution from noise.
These smoothed values of the observed $Q/I$ at the line center are used for all
further computations.
From Figure~\ref{slit-variation} we see that
the $Q/I$ at the line center shows more variation along the slit than at the blue wing peak.
This indicates the presence of varying horizontal magnetic fields and their possible role
in modifying the line center $Q/I$. These varying magnetic fields can in turn
be used to understand the observed line center $Q/I$ which are greater than the
theoretically predicted values. One possible explanation for this discrepancy could be
that observed line center $Q/I$
for $\mu > 0.35$ is enhanced due to the Hanle effect by these varying fields \citep[see also][]{mf94}.
This enhancement is very prominent in case of
the near disk center observations \citep[see][]{FS11}. However, in our case, it sets in for
$\mu > 0.35$ and
increases as $\mu \to 1$.
This is a clear evidence for highly structured, resolved, oriented magnetic
fields (predominantly horizontal) in the solar atmosphere.
However the dotted line in Figure~\ref{slit-variation} (for the blue wing)
do not exhibit the type of spatial fluctuations that is seen for the line
center (solid line). This is because the Hanle effect is absent in the wings.
We also note that the spatial variation close to the limb in the blue wing is not
really spectrally flat. The details regarding this will be
discussed in Section~\ref{depth-dependence}.

\subsubsection{The impact of temperature structure modifications on the
standard model atmospheres}
In the previous section we described the necessity of constructing a new model in order to obtain
a fit to the CLV of the Stokes profiles.
To this end, a new model was constructed by combining two standard models after modifying
their temperature structures at the desired heights. The new combined model thus constructed
will provide a fit to the CLV of the observed $Q/I$. The
physical consistency of the newly constructed atmospheric model with the modified temperature
structure has been checked by verifying that it satisfies hydrostatic equilibrium at all
heights.

Next we examine the fit to the CLV of the continuum intensity over a wavelength range spanning
from the visible to the infrared. The theoretical continuum intensity obtained using the new model
should fit the observed data
at all the limb distances and for a range of wavelengths.
Figure~\ref{clv-continuum} shows the limb darkening function computed using
the standard models and our new model
atmosphere $\overline{{\rm FALA}}$ + FALX
for a range of wavelengths and $\mu$ values. The theoretical values from different models
are compared with
the observed data from \citet{nl94}.
The dash-triple-dotted line represents the theoretical values from the new model
$\overline{{\rm FALA}}$ + FALX. We see that the best fit to the observations is
provided by the FAL-C model. The combined model though is successful in providing a CLV fit to the
observed $Q/I$ and satisfies the equilibrium conditions, it does not provide the best fit to
the observed CLV of the limb-darkening function and to the observed CLV intensity.

This leads
us to the conclusion that  it is indeed not possible to obtain a simultaneous fit to all
the various types of data with a single 1-D model atmosphere. One needs a different atmosphere for
each observable.
In search of a single model which satisfies all the observational constraints,
the next obvious step would be to use the two-component
modeling approach with appropriate mixing ratios as done in \citet{holandsten07}. In the section below
we discuss why we cannot adopt such a procedure in modeling the CLV of the Ca~{\sc i}~4227~\AA\ line.

\subsubsection{The two-component modeling approach}
\label{comparison}
In modeling the CLV observations of the Ca~{\sc ii} K line,
\cite{holandsten07} explored the possibility of constructing a
two-component model atmosphere. This was constructed by
mixing the results obtained from two standard model atmospheres
in appropriate ratios. Such a method was adopted by
making CLV plots of the Ca~{\sc ii} K line as shown in their Figure~1.
As seen from their figure, the original models FAL-X and FAL-C produce theoretical
CLV curves which fall respectively above and below the observed CLV curve of $Q/I$.
Hence they combine results from these two standard models with appropriate mixing ratios to
achieve the required fit.
In Figure~\ref{clv-plots} of the present paper we make similar plots
of the CLV for the Ca~{\sc i}~4227~\AA\ line.
As seen from Figure~\ref{clv-plots}, none of the standard model atmospheres
produce a theoretical CLV curve which falls above the observed CLV curve.
This does not allow us to apply the same kind of
two-component modeling procedure as described
by \citet{holandsten07}. This suggests that we need to go beyond 1-D modeling
in the direction of 2-D or 3-D
modeling to obtain a simultaneous fit to the ($I, Q/I$) at all the
limb distances. Such efforts are beyond the scope of this paper. However 1-D
models with modified temperature structures serve as a good initial step to
such elaborate computations. The failure of 1-D modeling approach does not preclude the
use of a given line profile for purposes like magnetic field determination.
To demonstrate this fact, in the next section, we perform observational analysis
of the Ca {\sc i} 4227 \AA{} line to
determine the field strengths for smaller $\mu$.

\begin{figure*}
\centering
\includegraphics[scale=0.47]{fig4a.eps}
\includegraphics[scale=0.47]{fig4b.eps}
\includegraphics[scale=0.47]{fig4c.eps}
\includegraphics[scale=0.47]{fig4d.eps}
\includegraphics[scale=0.47]{fig4e.eps}
\caption{Comparison between the observed (solid line) and the theoretical (dotted line)
Stokes profiles $(I,Q/I)$ at different limb distances. The combined model atmosphere
$\overline{{\rm FALA}} +{{\rm FALX}}$ is used to compute the theoretical profiles.}
\label{profiles}
\end{figure*}

\begin{figure*}
\centering
\includegraphics[height=6cm, width=16cm]{fig5.eps}
\caption{Center to limb variation of linear polarization at three chosen wavelength positions.
The model atmosphere used to obtain the theoretical profiles (dotted line) is the new combined model
$\overline{{\rm FALA}}$ + ${{\rm FALX}}$.}
\label{clv-new}
\end{figure*}

\begin{figure*}
\centering
\includegraphics[scale=0.9]{fig6.eps}
\caption{Variation of $Q/I$ values along the slit for each $\mu$ position (marked over the plots).
The solid and the dotted lines correspond to the $Q/I$ value at the line center and at the blue wing peak
respectively.}
\label{slit-variation}
\end{figure*}

\begin{figure*}
\centering
\includegraphics[scale=0.7]{fig7.eps}
\caption{Comparison between the  observed data for the CLV of continuum intensity
from \citet{nl94} for a range of wavelengths  and
the theoretical values from different
model atmospheres including $\overline{{\rm FALA}}$ + FALX. }
\label{clv-continuum}
\end{figure*}

\section{Determination of the field strength}
\label{depth-dependence}
In the present section we use an approach similar to that of \citet{bianda98,bianda99} to determine the
field strength at different limb distances. Since the observed $Q/I$ is influenced by so many factors
besides the magnetic field, it is imperative to apply {\it differential} techniques to isolate the
Hanle effect from the multitude of other effects. This can be done by using the wing polarization as
a reference, since it has been well established that the Hanle effect only operates in the line core
but is absent in the wings.

If we in Figure~\ref{slit-variation} compare $Q/I$ in the line core (solid lines) and in the blue wing
(dotted lines), we notice that the line core exhibits large spatial variations along the slit,
in contrast to the blue wing. Nevertheless, the blue wing polarization exhibits large-scale slow drifts
along the slit, which increase significantly as we approach the limb. Much of this can be explained in
terms of a geometric effect due to the limb curvature. Since the solar limb is curved while the slit
is straight, the limb distance (or $\mu$) will vary along the slit. This effect will increase in
significance as we get closer to the limb. It is an effect that is nearly identical for the line core
and wing (since the core and wing have nearly the same relative center-to-limb variations) and
therefore can be eliminated when forming the core to wing ratio. Similarly, any other unidentified
instrumental effect would ratio out. In principle there may also be non-magnetic effects of solar
origin, like spatial variations of the radiation-field anisotropy, which may be different between core
and wings and therefore would not fully ratio out (although they should be suppressed when forming the
ratio, since the non-magnetic fluctuations in the core and wings are not uncorrelated). However,
with our rather low spatial resolution and long integration times, these solar effects are expected to
be miniscule.

We therefore have strong reasons to believe that practically all the spatial fluctuations that we
see in the $Q/I$ core to wing ratio is exclusively due to magnetic fields via the Hanle effect.
Instead of directly using this ratio as our differential measure, we can scale it with the slit
average of the wing polarization, to express it in polarization units. This scaling is equivalent to
the assumption that the wing polarization should be spatially flat after all effects of limb curvature,
unidentified instrumental effects, and solar non-magnetic effects have been corrected for. We thus
correct the line core polarization amplitude with the following relation
\begin{equation}
 (Q/I)_{corrected}^{line\ center} = \frac{(Q/I)_{uncorrected}^{line\ center}}{P_b}\ {<P_b>},
 \label{correction}
\end{equation}
where $P_b = (Q/I)^{blue\ wing\ peak}$ for each pixel and $<P_b>$ is the spatial
average of $P_b$ along the slit. With this correction we plot in Figure~\ref{clv-slit} the CLV of
the spatially averaged $Q/I$ at the blue wing and the corrected $Q/I$ at the line center.
Each ``plus'' symbol in bottom panel of Figure~\ref{clv-slit} represents the value of $Q/I$
at each pixel corresponding to the line center. We notice large spatial variations along the
slit in the corrected $Q/I$ line-center data. This effect is
exclusively due to the magnetic fields via the Hanle effect. In order to find the field strengths
that contribute to such spatial variation, we follow the method used in \citet{bianda98,bianda99}.
We would like to note that in both these papers, for the data analysis,
the authors use observations taken at different periods. However in our analysis we
consider only one single set of observations and the variation of $Q/I$ along the slit
in these observations.
To this end we construct the envelopes (continuous lines in Figure~\ref{clv-slit})
to our data set, using the analytical relation
\begin{equation}
 \frac{Q}{I} = \frac{a (1-\mu^2)}{\mu+b}.
\label{empirical}
\end{equation}
This relation was first introduced by \citet{jos97} where $a$ and $b$ are the best fit free parameters.
For our studies we have chosen the same set of free parameters as given in \citet{bianda98,bianda99}.
From top panel of Figure~\ref{clv-slit} we see that the dashed line ($a$ = 0.33\%, $b$ = 0.02) gives a
good fit to the spatially averaged observed CLV profile in the blue wing.
In the bottom panel of Figure~\ref{clv-slit}
we use three different set of free parameters $a$ and $b$ to construct envelopes for
the line center data.
The envelopes constructed using the analytical relation given in Equation~(\ref{empirical})
represent the `non-magnetic value'
and all the values lying below this envelope are considered as the depolarized $Q/I$
values due to the Hanle effect. From our modeling efforts we know that the
magnetic fields cause an enhancement in the polarization value for $\mu > 0.35$
\citep[also see][]{mf94}. Hence this envelope
fitting method is good for $\mu \leqslant 0.35$ and becomes questionable for $\mu$ larger than about
0.35.
However the transition between the large angle scattering
and small angle scattering is gradual and smooth. For large $\mu$ we gradually enter into the regime of
forward-scattering Hanle effect, for which the kind of techniques developed by \citet{FS11} have to be adopted
to derive the field strengths. Full radiative transfer modeling is naturally needed for
intermediate $\mu$ values.
Only for smaller $\mu$ values it is possible to use a method that avoids the need for
radiative transfer. In this approach, we  first extract an observed depolarization factor via the
envelope method and then convert
this depolarization into field strength.

Thus we first determine the ratio between the line center $Q/I$ and the corresponding
envelope value.
This ratio represents the depolarization factor caused by the Hanle effect for each pixel.
The conversion of this factor into field strength is dependent on the choice of the envelope,
since it represents a
single observable, while the magnetic field vector is characterized by three parameters (its spatial
components). The magnetic field is therefore underdetermined, so a conversion cannot be unique,
but it is still meaningful
in a statistical sense, as explained in the following.

For photospheric spectral lines an interpretational model with a spatially averaged micro-turbulent
field distribution could be used to convert Hanle depolarization into field strength
\citep[][]{sten82, jos94}, because the absence of $U/I$ polarization in combination with insignificant
spatial variations (at resolved scales) in $Q/I$ made such a micro-turbulent interpretational model
unavoidable \citep[see also][]{jos13}. The situation is however entirely different for strong
chromospheric lines like the Ca {\sc i} 4227\,\AA\ line, which always exhibits large spatial line-core variations
in both $Q/I$ and $U/I$, like those in Figure~\ref{slit-variation}. As we have spatially resolved these
variations, they should ideally be interpreted in terms of resolved, oriented fields rather than
angular distributions. However, since the field vector is underdetermined by the single depolarization
factor, we need to eliminate the ambiguity by using the statistical approach, dealing with each
depolarization factor as if it were obtained through averaging over an ensemble of field elements.
This approach will give field strength values that are meaningful as averages in a statistical sense.

Vertical fields are immune to the Hanle effect, depolarization can only occur if the field has a
substantial inclination with respect to the vertical direction. Horizontal fields give the largest
depolarization. If we assume the fields to be horizontal, but with orientations that are random in
azimuth angle, and let the Hanle depolarization be determined by an ensemble average over such a field
distribution, then the field strengths that we extract from this model can be considered to represent
{\it lower limits} to the true average field strength (since there may exist less inclined fields
that are less ``visible'' to the Hanle effect).

Chromospheric fields are expected to be largely horizontal, forming a ``canopy'' over the
underlying photosphere. The Hanle depolarization factor $k_H$ for a horizontal field distribution
with random azimuths can be written as \citep[][]{sten82, jos94}
\begin{equation}
 k_H = 1 - 0.75\sin^2 \alpha_2,
 \label{depol}
\end{equation}
where the Hanle mixing angle $\alpha_K$ is given by
\begin{equation}
 \tan \alpha_K = \frac{K B}{B_0/k_c^{(K)}}.
\label{mag}
\end{equation}
$B$  is the field strength to be determined, $K$ = 1 or 2,
$k_c^{(K)}$ is the collisional branching ratio for the 2$K$-multipole and $B_0$ is the
characteristic field strength for the Hanle effect.\\

Figure~\ref{histogram1} shows the histograms of the field strengths obtained when using
Eqs.~(\ref{depol}) and (\ref{mag}) for all pixels along the spatial direction.
By definition, a depolarization factor should be less than or equal to unity, otherwise
it is unphysical. However, some points give an unphysical depolarization factor, both because
there is scatter of the $Q/I$ values due to measurement noise, and because the chosen
envelope may be too low. In such cases the field strength used for the histograms in
Figure~\ref{histogram1} is set to zero. The number of such zero field points depends on the
choice of  envelope and increases as we move away from the limb because of the increasing
contribution from the forward-scattering Hanle effect.

Figure~\ref{histogram1} shows how the field-strength fluctuations along the slit vary
with different limb distance. For the derivation of the CLV of the average field strength,
which is shown in Figure~\ref{field}, we do not average the field-strength histograms of
Figure~\ref{histogram1}, because they are affected by measurement noise in a non-linear way
(including the truncation used for the unphysical values), but we instead average the measured
$Q/I$ along the slit (causing the Gaussian instrumental noise to get greatly suppressed), and
then convert the average $Q/I$ to field strength. Since the height of line formation increases
with decreasing $\mu$, the $\mu$ variation displayed by Figure~\ref{field} may be interpreted in
terms of a height variation of the field. In view of the limited statistical sample and the crudeness
of the interpretational model the minor variations with $\mu$ in Figure~\ref{field}, which
are similar to the ones obtained by \citet{bianda98,bianda99}, are not significant but are
compatible with approximate constancy of the average field strength over the height range covered
by our $\mu$ range.

Note that we have limited the $\mu$ range in Figure~\ref{field} to 0.1 - 0.35, because as
mentioned before the envelope method is not applicable for larger $\mu$ values.
Note also how the derived mean field strength depends on the choice of envelope.
In spite of these uncertainties, the values are generally limited to the range 6 - 10\,G.
We cannot choose envelopes significantly lower than the one represented by the
solid line (in the bottom panel of Figure~\ref{slit-variation}),
because one would then get an excessive number of unphysical depolarization factors.
Therefore the 6\,G value can be seen as representing a kind of lower limit for the average
field strength.

\begin{figure*}
 \centering
 \includegraphics[scale=0.5]{fig8.eps}
 \caption{CLV of $Q/I$ at the blue wing PRD peak (top panel) and at the line center (bottom panel).
Plus sign represents the $Q/I$ value at each pixel along the slit in the bottom panel and
spatially averaged value of $Q/I$ in the top panel.
The solid, dotted and dashed curves are obtained
using the empirical relation given in Equation~(\ref{empirical}). The corresponding value of the free
parameters $a$ and $b$ are indicated in the figure.}
  \label{clv-slit}
\end{figure*}

\begin{figure*}
 \centering
 \includegraphics[height=18.0cm,width=14cm]{fig9.eps}
 \caption{Histogram of the field strength at different $\mu$ positions. Field
strengths are computed for each depolarization value in the spatial direction. Different
panels along the row for each $\mu$ correspond to field strengths obtained using different envelopes.
The solid, dotted and dashed lines respectively correspond to the solid,
dotted and dashed envelopes in Figure~\ref{clv-slit}.}
 \label{histogram1}
\end{figure*}

\begin{figure*}
 \centering
 \includegraphics[scale=0.6]{fig10.eps}
 \caption{Mean value of field strength (G) derived from averaged $Q/I$ value along the slit.
The solid, dotted and dashed lines correspond to the mean field strength derived from the
corresponding envelopes indicated in Figure~\ref{clv-slit}.
}
\label{field}
\end{figure*}

\section{Conclusions}
\label{conclusion}
To understand the depth dependence of various physical quantities in the Sun,
like the magnetic fields, it is important to model
the CLV observations of suitable atomic and molecular lines.
In this paper we have attempted to model such CLV observations of the well
known Ca {\sc i} 4227 \AA {}
line. In our approach we take into account the effects of
partial frequency redistribution (PRD) and radiative transfer.
The observations of this line were carried out in quiet regions
on the Sun at 14 positions starting
from the limb up to the disk center on October 16, 2012 at IRSOL in Switzerland.
This line has the largest degree of linear polarization in the visible region of the
Second Solar Spectrum
and can be modeled by considering a simple two-level atom picture.
When trying to model this CLV data we find that none of the standard atmospheric models,
attempted by us,
like the FAL-F, FAL-A, FAL-C, and FAL-X could simultaneously fit
the observed $(I,Q/I)$ profiles at all the limb distances.
To model the CLV of the line center intensity we need FAL-F model which is the
hottest and to
model the CLV of the linear polarization at line center we need the coolest model FAL-X.
In order to obtain a fit to the observed Stokes profiles, modifications in the temperature structure
of the standard models become necessary. With suitable modifications in the desired height range,
we constructed $\overline{\rm FALA}$ and later combined it with FAL-X.
While the $\overline{\rm FALA}$ model gives a good fit to the PRD peaks, the
FAL-X gives a good fit to the line center. The combined model has
the temperature structure of
$\overline{\rm FALA}$ up to 400 km, and that of
FAL-X in the upper layers. This new combined model atmosphere
gives a good fit to the entire $Q/I$ at all values of $\mu$.
Also in modeling efforts we found that the Hanle
effect not only depolarizes the line core of $Q/I$
(which is true for smaller $\mu$'s)
but also enhances the line core $Q/I$ for larger $\mu$ values. This might
be due to the highly structured horizontal magnetic fields in the solar atmosphere.

Though the new combined model provides a fit to the CLV of the observed $Q/I$,
it fails to reproduce the
observed CLV of the continuum limb-darkening function and the CLV of the observed
line core intensity.
This failure of 1-D models in order to simultaneously fit the observed
$(I,Q/I)$ CLV profiles do not restrain the use of the Ca {\sc i} 4227 \AA{} as
a tool to map the magnetic fields. To support this claim,
we carried out observational
analysis to determine field strength using
the Ca {\sc i} 4227 \AA{} for smaller $\mu$ values.

To conclude, it appears that no single 1-D atmosphere can completely
provide a good representation of the actual solar atmosphere.
This shows that the solar atmosphere has a far more complex structure.
To simultaneously satisfy the various observational constraints it is therefore
unavoidable to go beyond such 1-D models - a difficult problem that needs to be approached step by step.
This conclusion is not at all a technical failure
meaning that our inability to obtain a simultaneous perfect fit to the CLV of the ($I$, $Q/I$)
has nothing to do with the weakness of our approach or the method followed in using
1-D solar atmospheres. Instead it is a ``profound failure'' indicating that the atmosphere of the
Sun has such a complexity that it is not possible to represent
it in terms of a single 1-D atmosphere. It could mean that the use of 1-D models
for interpretations of the Second Solar Spectrum may give results that are
physically incorrect (since they do not represent solar conditions),
although the results may formally be mathematically correct. However, 1-D modeling efforts
may still provide a guideline to the more systematic and sophisticated modeling efforts.

\begin{acknowledgments}
We are grateful to  Dr. Han Uitenbroek for providing us with his
realistic atmospheric modeling code.
Research at IRSOL is financially supported by State Secretariat for
Education, Research and Innovation, SERI, Canton Ticino, the city of
Locarno, the local municipalities,
the Foundation  Aldo e Cele Dacc\`o
and the Swiss National Science
Foundation grant 200021-138016. RR acknowledges financial support by the
Carlo e Albina Cavargna foundation. We are grateful to the referee for
very detailed and useful comments which helped in improving the paper
substantially.
\end{acknowledgments}

redpajama_set_name: RedPajamaArXiv


I thought I was fit, so going to a session of an American workout scheme called CrossFit in St Ives was a rather humbling experience.
It is tailored for people of all ages and fitness, and is used extensively by the US military but has only recently crossed the Atlantic.
CrossFit South is a training session that involves exercises that can be done anywhere, such as press ups, sit ups and squats. "It's based on gymnastics and Olympic weight lifting, a circuit that's different each time," said instructor Lissette Bonin-Casey, 41, from St Ives. "It can be used to keep anyone fit, from an 80-year-old to a child, for sports or just general fitness. The idea is that we tailor it so that if you're injured you can still come and get a good workout.
"All the movements are based on things you can do and the exercises are different each time. You can't train for it because it changes every week and your body can't get used to it so it's constantly improving your fitness."
The CrossFit session I attended started with a quick warm up session of dodge ball before we moved on to press ups, sit ups, squats and stretches. We then did timed sessions whereby each person had to do as many sit ups as they were able to whilst using proper technique in 30 seconds. Everyone then announced their score before another 30 second round in which you had to score as high as the first, and this continued for six or seven rounds. The same thing was then repeated with squats before a few more exercises were practiced.
The class then did a circuit (pictured) that included five exercises - steps downs with a jump in between changing, geckos (a press up whereby when you are down you must raise one knee to touch your elbow, then repeat with the opposite knee on the next one), squats with a heavy ball that you have to throw when going up, deadlifts with a bar that you must push above your head and squats where you must pick a weight up off the floor and raise it to your shoulders. The class did one circuit including all the exercises with a minute of each, and a second circuit with 20 seconds of each.
The USA has about five to ten affiliates that practice CrossFit classes in every state, and there are currently over 25 in the UK, with two new ones opening this year alone. It became popular in the USA shortly after Greg Glassman fromSanta Cruz, California, launched a website in February 2001 with daily CrossFit workouts. He soon picked up interest from police, firefighters and the military, who all now use it as a training schedule.
Bonin-Casey's husband Pat, 36, who serves in the Marines, described it as "a constantly varied programme with functional movements executed at a high intensity."
The Bonin-Caseys started teaching CrossFit sessions last April at the Ivo outdoor centre. They spent a fortnight in America getting qualified in San Francisco and Oakland, California. "It's been fun since we started doing it and the group has regulars that have become hooked and come week in week out and have supported us really well," said Lissette Bonin-Casey, who works as a teacher part time. "It's getting more popular and I think it will this year. As it's all coached this makes a massive difference to circuit training.
"There's more focus on your fitness and technique and safety is paramount. Anyone can come from total beginners to proper athletes."
The class who came to the session I did certainly seemed to get a good workout. Many of them have been coming since the Bonin-Caseys started it and have kept coming since then.
Mark Thompson, 43, is a swimming development officer from St Ives. "I find it hard work as I regard myself as pretty fit but this improved my fitness twofold. I love it and I don't do any other training now," he said. "I needed something new to train with and this has been brilliant as we don't know what we will get and learn new techniques and exercises every week."
"I guess you could call it enjoyment, I have definitely seen my fitness improve because of it," said environment agency worker Karen Paterson, 36, from Houghton.
"It's good fun and quite enjoyable and I've definitely seen my fitness improve vastly," said software engineer Jamie Kirk, 35, from Abbots Ripton. "I was circuit training but you get used to that whereas this is different each week."
Darran Gray, 33, from St Neots, is a teacher who made it his New Year's resolution to come. "It's hard work and it was nice that she adapts it because I have a bad back and it was changed for me so I will definitely be coming back. I could feel it and I'm sure that if I continue doing it then I'll get fitter."
The CrossFit class was certainly hard work, and I could still feel the after effects in the morning. It was fun to be doing the exercises with other people and the trainers made sure you do the exercises properly and get the correct, safe technique. It certainly seems a good way to get fit and the way the classes work make it suitable for anyone.
CrossFit South classes run from 6pm to 7pm on Mondays during term time at the St Ives Parish Church Hall on Ramsey Road. Classes cost £5 with no joining fee and the next one will be on January 26.


text:
Local News > Three cops promoted to superintendent
Three cops promoted to superintendent
Three chief inspectors within the Royal Virgin Islands Police Force were recently promoted to the rank of superintendent, the Police Information Office announced recently. Selwyn Rock and Dariel Robinson were …
Continue reading "Three cops promoted to superintendent"
by Alva Solomon | January 15, 2023
Three chief inspectors within the Royal Virgin Islands Police Force were recently promoted to the rank of superintendent, the Police Information Office announced recently.
Selwyn Rock and Dariel Robinson were promoted to the rank of superintendent in charge of the Territorial and Operations divisions, respectively.
Their promotions are effective immediately. Messrs. Rock and Robinson had been acting in the posts for more than a year, the police noted. Meanwhile, Paula Alleyne was promoted to superintendent in charge of the Crime Division, but she will continue to act in the post until the promotion takes effect on July 15.
The promotions followed recommendations made to Governor John Rankin by the Police Service Commission and ratified by the National Security Council, according to the Police Information Office.
Police Commissioner Mark Collins congratulated the officers and encouraged others to prepare for upcoming opportunities. "The [police force] takes pride in being able to grow our numbers not only at the bottom with new recruits, but at the top as well, thus opening opportunities for other officers to move up in rank," he said.
"We have now confirmed three superintendents, which would make way for promotions to the chief inspector rank, for which the process is being finalised. I urge all who qualify to prepare themselves for possible advancement."
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redpajama_set_name: RedPajamaCommonCrawl


Smart real estate investors know how critical it is to have an effective lead follow up process. Danny Johnson joins us today to share some advice on this super important topic. Generating great leads is important…but it's all for nothing if you don't follow up on those leads! Check out this FlipNerd Expert Tip.
Mike: Hey, it's Mike Hambright from FlipNerd.com and we have a quick Expert Tip to share with you from Danny Johnson who's going to share some advice on the importance of lead follow-up.
Danny: Hey Mike. Thanks for having me on. Lead follow-up is super important. Especially in this day and age where there are a lot of real estate investors going after deals and you might find yourself talking to a seller of a house that is also talking to some other investors. That's always happened in the past, will happen always in the future.
But the people that follow up are the ones that get most of the deals. When you go and look at a house and you do some analysis and make an offer on it to buy the house, a lot of times the seller isn't going to want to sign a contract with you right away. Right? Except for the super motivated ones. Those are always the great ones because you walk away from there victorious and head to the title company and take your wife to dinner that night and everything.
But most of the time a seller is not going to want to sign right away. They need to think about it or they have some other investors coming. And you can try to close the deal then and put some pressure on. But that's just not my style. I feel that sort of puts some negative on me from the seller's point of view, that I was kind of pushy or something like that. And there's ways to do a little bit of pushing without seeming that way.
It's definitely not by telling somebody, "Well this contract is only good for two hours." That's just bad. I've seen people say and do things like that and it's just crazy to me.
So the important thing is follow up because if they're not going to sign with you right away, most likely the other investor that's coming later, they're not going to sign with them either. So you've got to have a system for following up.
So what I typically do is I'll call them later the same day and just ask if they've thought more about my offer, if there are any questions. And then the next day I'll call again. And then from there you spread it out a little bit more if they haven't made the decision yet. But you have to continuously call them over time. So you can make it spaced out a little bit more. But typically real motivated sellers are going to make the decision within a day or two.
So if they're not super motivated it doesn't mean to stop calling them, just put it spaced out longer. Really you want to continue to do that until they tell you, "Stop calling me" or that they've "already sold it" or "yes come buy my house." The thing is they might be busy. They might be thinking of other things they want to look at doing. Maybe they have an uncle that wants to move into the house. All these things that they might like your offer but they have some other things they want to think through.
And if you're not top of mind when they do decide to go ahead and sell for cash quickly you're not going to get the call. But if you're calling them all the time they're going to say, "I'm going to call Danny now. He's been calling me." It's awesome. It really works.
Please note, the views and opinions expressed by the individuals on this program do not necessarily reflect those of FlipNerd.com or any of its partners, advertisers, or affiliates. Please consult professionals before making any investment or tax decisions, as real estate investing can be risky.


With the announcement of candidates for Durg and Korba late Monday evening, the Congress has completed ticket distribution in all 11 seats of the state.
The Congress has fielded women candidates, including a former MLA, in two key constituencies – Durg and Korba in Chhattisgarh for the April-May Lok Sabha polls.
Former MLA Pratima Chandrakar will take on the BJP's Vijay Baghel, a Kurmi leader and former MLA, from Durg Lok Sabha seat.
Jyotsna Mahant, wife of Assembly Speaker Charandas Mahant, has been fielded from Korba against BJP's Jyotinand Dubey.
They said Mahant's work in the region would help his wife's poll prospects.
Chandrakar was MLA from Durg Rural seat in 2008 but lost the 2013 Assembly polls.
In the 2018 Assembly polls, she was replaced from the seat by sitting MP Tamradhwaj Sahu.


It all came down to me.
The one who followed the rules, never went looking for trouble – I kept to myself. I just wanted to take care of my family. To not constantly look over my shoulder, worried about the things that went bump in the night.
I just wanted to survive.
But that wasn't meant to be.
As luck – or fate, or something – would have it, the trouble found me.
I followed a rabbit through the wreckage of a half-ruined world to get back what was mine, and wound up at the end of it.
But there's nothing magical about it.
Before we get into this review, let me just say this: I've long been a Christina C. Jones fan but honey! After Wonder?! I need to increase my dues to the CCJ fan club. Someone send me the new invoice!
Wonder by CCJ is my catnip. It's a dream. I'm a huge fan of post-apocalyptic stories, TNT's Last Ship was one of my favorite shows and I'm STILL upset that we won't get a new season this year. As soon as I heard this novel would have a dystopian Alice In Wonder-esque theme, I knew I would love it.
And love it I did.
The main character Aly lives is a post-apocalypse world where the lines are distinct; power and control are paramount and the rich get richer while the poor try to get by.
Aly is pretty alone in the world; her only remaining family is her grandmother and her sister, Nadia. Aly follows the rules, is mindful to stay out of everyone's way and tries to take care of her family the best way she knows how. She doesn't get in trouble but trouble finds her when his sister goes missing, presumably in the worst part of town and she must find a way to get her back.
Enter Maddox, a loyal enforcer of sorts to his leader, Ches, who is questionable, to say the least, but someone he holds near. Maddox doesn't plan to save a stranger's life but when Aly finds herself in a bit of trouble he can't rightfully leave her to fend for herself. Aly's decision to go after her sister and Maddox's decision to save Aly changes everything they were once certain they knew.
Without giving too much away because you all know how I go LOL, from here we are swept up in a tale that is reminiscent of Alice in Wonderland but told in a way that that is still distinctly CCJ. I loved the play on the names and the introduction of intriguing characters. There's not one character here that I didn't want to know more about and honestly, that's pretty rare for me. My hope is that we get to visit this world again because I simply couldn't get enough.
CCJ weaves a sweeping tale of power struggles and disillusions but most of all courage and love. Did I forget to mention how much I loved the connection between Aly and Maddox?! Tuh! Forgive me.
I feel like Wonder was written for me; the girl who loves fairytales, is inquisitive about all of the what if's, and believes that in any world, a deep, authentic connection should always be cherished.


Read how one Vietnamese family celebrates New Year's in a uniquely Vietnamese way—preparing and eating traditional foods, observing special traditions, watching fireworks and a dragon dance, and sharing good times with family members.
Spring is coming, the period of time to which I always aspire. It means that the New Year is also coming soon. That's the first day of lunar calendar, around the end of January and the beginning of February in Solar calendar.
Regardless of age, society class, or living conditions, every Vietnamese family celebrates the New Year in the same traditional way. It's considered to be the most important and wonderful holiday in my country, since that is the time for people to leave their haplessness in the back and get their fortune for the New Year. Similar to other houses, my family has always bustled in preparing and greeting for the New Year.
That was the preceding day of the New Year, and it was also the busiest day in my house. My mother went to the supermarket early in the morning and came back with a bunch of food. From then, the clatter of dishes and pans and the sizzle of food that has been fried were far resounding incessantly until late evening.
At any place of the house, you could even hear the noisy boil on the stove or the scrunching of my mother's spoon scratched on the pan. You could also smell the burn of coconut jam, which was being made by my sister.
"Why do you always burn it?" I shouted.
"That's the way I like," she said and laughed at me.
I loved her jam so much, but she was always burning it until the white coconut jam became the yellow jam. It was terrible! At noon, the puff of smoke and the mixed scent from various kinds of food started spreading over my house.
After that, certainly, there were my father's footsteps clattering on the floor. He left his half-painted walls in the living room to go into the kitchen and grumble to my Mom. "Your smoke is disturbing me."
In fact, he just wanted to look around the kitchen room with many kinds of food on the table. Then he smiled contentedly when seeing my mother cooking next to the tiny crackles of burnt firewood in the stove and the bright red fire, which were blazing up the kitchen.
At the end of the day, when everything was done, my house became brilliant with the colorful balloons, ribbons, and flowers. However, you shouldn't sit next to the walls in the living room because the layer of new paint was still sticky and would adhere on your clothes. Moreover, the smell of paint was very strong at the end of this day.


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WA tourism operators cry for help as lockdowns hit on two fronts
By David Prestipino
July 1, 2021 — 12.00am
Tourism Council WA said "tens of thousands" from interstate have cancelled holidays to WA
"Hundreds of thousands" of West Australians likely to cancel trips north and south of WA
United Nations report said tourism slump from COVID-19 to cost $5.3 trillion
West Australian tourism operators have called for financial support after forecasting huge losses from this week's snap four-day lockdown and are bracing for more if it is extended beyond Friday.
Premier Mark McGowan said on Wednesday any government assistance would hinge on whether the lockdown continued beyond Friday into WA's school holidays.
Seashells Resort said each of its four properties were impacted first by the NSW then Perth/Peel lockdowns.
But the state's peak tourism body said businesses had already suffered from "tens of thousands" of interstate visitors cancelling holidays after schools over east finished a week earlier.
"They have taken financial hits on two fronts after the state's border was closed to effectively the rest of Australia and holidaymakers from Perth and Peel are now locked out of popular winter school holiday destinations up north and down south," Tourism Council WA chief executive Evan Hall said.
Tourism operators and associated businesses in the North West were hardest hit, with the majority of their annual revenue coming in July.
Compounding their losses were additional costs in sourcing supplies and staff for upcoming tours, and refunds that would now be returned.
"These tourism businesses are losing their income in peak period and its grossly unfair to put the cost on a very small group of people."
Tourism Council chief executive Evan Hall
Perth hotels and tour companies would also suffer, losing visitors from the east coast who would normally spend a few nights in the capital either side of trips across WA.
"There are a lot of small groups, families and couples that book extended, high-end tours to regions such as the Kimberley and the tourism business is with them the entire time – driving, camping, cooking meals – it's a real high level of service," Mr Hall said.
"These are the sorts of things that Perth people generally don't pay for.
"The Kimberley is very, very seasonal and a lot of businesses are only able to get customers from out of the state ... to lose this month of July, after going through what it's gone through the past 18 months is just devastating."
Mr Hall said "hundred of thousands" of visitors would also normally empty out of Perth into the regions for the school holidays.
"A majority of these people start their trips a day or two earlier [than this Saturday] and I can tell you they are already cancelling as they are scared they will lose their money," he said.
"We urge people to modify their holiday as a lot of these businesses in the regions – from your mini golf in Margaret River to camel riding in Broome – they've geared up, staffed up, bought supplies and now suddenly it's all wiped out."
The Tourism Council wants the WA government to provide support packages well above the $2000 businesses could access during the lockdown in April and waive the "small fortune" in government fees for recreational, park and vehicle permits, booking authorisations and insurance.
"It has to be commensurate with the losses these business are suffering," Mr Hall said, citing NSW's recent assistance package of up to $10,000 for impacted businesses.
Sean Blocksidge's tour company is consistently rated number one for Margaret River tour experiences on Tripadvisor.
"And it can't be limited to the businesses in the lockdown area; these losses hit across WA.
"The true cost of this lockdown is actually paid for by very few people ... these tourism and other small businesses are losing their income in peak period and its grossly unfair to just put the cost on a very small group of people."
Margaret River Discovery Company owner Sean Blocksidge had all of his tours cancelled this week but was offering full refunds and still receiving bookings for later this month.
"A few weeks ago I was fully booked with tours for this week but as of Tuesday afternoon every single tour was cancelled due to lockdown restrictions," he said.
"That's zero income unfortunately. It'll be the same for a lot of hospitality/tourism/entertainment businesses across the country. There's no safety net this time."
Mr Blocksidge hasn't charged cancellation fees since COVID-19 began, and said among this week's bad news was the good news that six people had booked tours for July.
"I think it's important that people have the confidence to book and plan holidays and know they won't be out of pocket if plans change beyond their control," he said.
Seashells Broome had a raft of cancellations from NSW when the state first locked down but was able to rebook a majority of them with Perth people for the WA school holidays.
General manager Deb Williams said the company was doing everything it could to accommodate clients to re-book or provide full refunds to those who couldn't travel or change dates.
"Most of the cancellations we received in Broome from the NSW lockdown were filled with people already in town or already staying with us, wishing to extend their stay to avoid the lockdown," she said.
"For the Perth lockdown we have been able to extend our current guests and take additional bookings, with about 30 per cent occupancy loss this week for Seashells Broome."
Ms Williams said bookings from July 3 onwards were holding for now and she hoped Perth and Peel would come out of lockdown on Friday.
Tourism WA acting managing director Derryn Belford said it would engage regional organisations to encourage locals to holiday and spend their money in WA once lockdown ended.
"I know many are needing to work through cancellations, refunds and postponements, all of which present many challenges, physically and emotionally," he said.
"We are also in market with other states and territories, and New Zealand, so when people are ready to book a holiday again, WA is at the top of their list."
A United Nations Conference on Trade and Development report released on Wednesday said the slump in tourism from COVID-19 would cost the global economy more than $5.3 trillion for 2020 and 2021, as an uneven vaccination rollout crushed countries dependent on international visitors.
David Prestipino writes about sports and lifestyle for WAtoday.Connect via Twitter or email.


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Review: $1400 Samsung Notebook A Great All-Rounder
Web Development July 4, 2017 ArchiveIT HardwareReviews
Product Rating9
Editor Rating9
The R590 is a powerful notebook aimed at users who want a 15-incher that delivers. We take a look at what this $1400 model brings to the table.
Though the likes of Dell offer the option of colourful lids and designs, in general PC manufacturers shy away from bold colours. Anything grey, black, or brown-ish goes down well, as has white in times past. Samsung, however, is unusual in making its laptops more than a little colourful.
For the R580 and R780 the colour of choice was red, but the new R590 opts for a fetching deep blue instead.
Aside from the change of colour, the R590's chassis is more or less identical to its predecessors. Both the lid and body are punctuated by a pretty swirling pattern, and the touchpad is flanked by small blue LEDs on each corner. One difference, however, is that the R590 has a seamless, flat bezel surrounding the screen. This looks cool, but does suffer reflections worse even than the standard reflective finishes of most laptops.
In general the design is an attractive one. The R590's 2.6kg weight isn't too hefty and it's no thicker than the majority of laptops in this segment. Our only pressing criticism, a common one as it happens, is that the glossy finishes are very fingerprint prone – a problem not present on the Q530.
Where the R590 excels is in its generous specification. Despite actually costing less than the Q530, it boasts a faster 2.4GHz Intel Core i5 processor. Added to the 4GB of RAM, 500GB hard drive and a capable 1GB Nvidia GeForce GT 330M graphics card, and the R590 ticks a lot of useful boxes. Also under the features column is the now obligatory 802.11n Wi-Fi, Bluetooth 3.0 and Gigabit Ethernet, not to mention a 1.3-megapixel webcam.
You're unlikely to be left wanting for connectivity, either. There are four USB ports, one of which doubles as an eSATA port, while another offers standby USB charging. HDMI and VGA are present, too, and the R590 is unusual in retaining a 34mm ExpressCard slot – useful if you want to add USB 3.0 support, for instance. Also included, but not shown above, is a memory card slot that's on the front edge.
Samsung tends to use a lot of common components among its laptops, which is no bad thing as the keyboard on the R590 is just as good as its other machines. As is the modern fashion the keys are isolated, and there's also a numeric keypad for making quick calculations. Key actions are sharp and precise, and don't suffer the shallowness often attributed to isolation keyboards.
However, also in common with other Samsung laptops of late, the R590's touchpad is positioned to the right of the Spacebar. Consequently, when typing, your palm tends to rest on the edge of it, jogging the cursor and often causing errors. It seems a trivial, minor problem at first, but the reality is a good deal more irritating. If you're concerned, it's worth giving the R590 a test run before purchase.
Aside from getting in the way, the touchpad is very good. It's a good size, has a nice, low-friction surface and its buttons are precise and easy to located. We're not sure the four LED lights that demark each corner add much, but they don't hurt.
As mentioned earlier, one of the side effects of the fetching seamless bezel is the 15.6-inch screen is quite reflective. Not a problem if indoors, where this machine is likely to spend most of its time, but not a positive trait in the great outdoors. In its element, however, the display is impressive. Its 1,366 x 768 resolution is nothing outstanding, but it's vibrant and reveals plenty of detail in videos and photos.
You'll need a decent set of headphones or speakers to hand, however, as the R590's speakers are thoroughly mediocre. They just about pass muster for watching online video clips and maybe the odd TV show, but for anything else they lack the mid-range clarity for genuine enjoyment or immersion.
In practice, the R590 is the kind of machine that can genuinely replace a desktop. It won't break sweat with day-to-day computing tasks, and is fast enough to tackle more demanding tasks like photo editing and video encoding. It's an all-round workhorse.
This applies equally to games, where the R590 also performs well. It registered good results in both our tests, though the more demanding Stalker: Call of Pripyat demonstrates you'll need to stick to medium detail settings for the latest games. Less demanding titles, on the other hand, won't pose any meaningful challenges.
Battery life isn't very long, registering around three hours of productivity, but a fair way short of two of DVD playback. Reduce the brightness and you'll get a little more than this, but the reflective screen demands a slightly higher brightness than other laptops.
Mediocre battery life is easily forgiven, however, as in every other respect the R590 is a very good laptop and a great deal to boot. Some may find the colourful finish, and its all-round glossiness, off putting, but if not then it's definitely worth a look.
A powerful, flexible and good-looking laptop, the R590 can service all your computing needs without breaking the bank.
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Sierra Rep takes on Hitchcock's '39 Steps' with recycling cast
Few plays recycle a handful of actors in and out of so many versatile roles as in Sierra Repertory Theatre's "The 39 Steps." The end result of using four players in dozens of roles in the stage adaptation of the early classic Alfred Hitchcock film is light-hearted stage filled with unexpected comedic approaches.
The Tony Award-winning comedy plays at SRT's East Sonora stage through July 1.
The cloak and dagger play involves the adventures of mild-mannered hero Richard Hannay who is plunged into a maze of murder, romance and intrigue in pre-war London. Hannay (played by Toby Miller) wanders out for an evening at the music hall and finds himself suddenly entangled with a mysterious young woman with a desperate secret that could decide the fate of Europe. When she's murdered in his flat, he's yanked into a mysterious world of spies and double agents. Falsely accused, he is chased from trains through the British country side as he tries to clear his name and save his country from a sinister plot.
While multi-character players Jim Shine, David Thornton and Laura Cable do a good job as quick change artists, switching accents and voices with parts, it is Thornton is who masterfully pulls off the demanding differences in his obtuse characters. Count on antics of Shine - who exaggerates roles ofs several women for laughter - to keep things interesting too.
Cable is convincing in her roles but her thick accent trips her words at times.
The scene changes with minimal props are quick and clever and keep things interesting. The audience visits a railroad station, country inn, lake side and inside the mansion Alt Na Shellach, which yields surprises Hannay didn't quite anticipate in this slightly off-the-wall farce.
The audience is quick to laugh during the use of cutouts on wires to cast shadows on a silk screen behind the actors. Yes, the bi-plane gunning for Hannay in one farcical scene is stolen from a scene in another Hitchcock thriller, North by Northwest.
One Modestan in the opening night crowd who rarely attends community theater smiled during the play and commented that "it was cute."
We'll give SRT the benefit of the doubt that future performances will be accomplished in a cooler venue. If the air conditioning unit was working you couldn't tell from those fanning themselves with programs. In all fairness, temperatures had hit 99 in the foothills that afternoon.
The 39 Steps is worth the drive and an evening of laughs. Shows are offered Thursday and Friday begin at 7, Saturday evening performances are at 8 and Wednesday, Saturday and Sunday matinees begin at 2. Ticket prices range from $24 to $30. The show is rated PG, appropriate for all audiences ages 10 and up.
For more information or reservations, call Sierra Rep's box office at 532-3120, visit www.sierrarep.org.
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Is Leggett & Platt a Buy Under $40?
Leading engineering components manufacturer Leggett & Platt (LEG) generated record sales of $1.3 billion in the third quarter. However, since the company's financials continue to be negatively affected by supply...
By Imon Ghosh December 27, 2021
Leading engineering components manufacturer Leggett & Platt (LEG) generated record sales of $1.3 billion in the third quarter. However, since the company's financials continue to be negatively affected by supply chain constraints and inflationary pressure, is the stock worth betting on at its current price level? Read on.
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Diversified manufacturer Leggett & Platt, Incorporated (LEG), in Los Angeles, manufactures and produces bedding, furniture, residential furnishings, and other various engineered components. A substantial increase in prices for raw materials, strategic acquisitions, and a return to normal seasonal levels of demand in Europe helped the company report record sales growth in the third quarter.
Its shares have soared 4.1% in price over the past five days. However, LEG's stock is down 8.1% over the past month and 14.4% over the past three months to close its last trading session at $39.57.
Although LEG's resilient business model and sales growth across diverse business segments bode well for the stock, several macroeconomic headwinds, including high raw material prices, elevated freight costs, and supply chain constraints, could be concerning. In addition, the company's narrowed full-year 2021 guidance and declining volumes across all business segments could hamper its growth and hurt investor sentiment.
Here is what could influence LEG's performance in the upcoming months:
Macro Headwinds
LEG continues to experience multiple macro challenges that have negatively impacted the company's sales volume and EBIT in its last reported quarter. Its volume fell 6%, due mainly to supply chain constraints hampering the Bedding and Automotive markets. In addition, challenges related to foam chemical shortages and labor availability could hurt the company's earnings and revenue. Furthermore, higher freight costs and raw material-related price increases due to rising inflation could threaten its growth in the near term.
Tepid Quarterly Performance
During the third quarter, ended November 1, 2021, LEG's sales rose 9% year-over-year to $1.32 billion, driven by a 13% increase in trade sales in the Bedding Products segment and a 12% increase in the Furniture, Flooring & Textile Products segment. However, the company's gross profit declined 5% from the prior-year quarter to $256.1 million, while its EBIT decreased 4%. Its net earnings fell 9% year-over-year to $97.2 million, while EPS declined 10% from the prior-year quarter to $0.71.
LEG's net cash from operating activities came in at $50.1 million for the quarter, compared to $261.3 million for the same period last year. And its adjusted EBIT margin under Specialized Products segment fell 550 basis points year-over-year to 9.5%.
LEG's 9.46x forward EV/EBITDA ratio is 7.6% lower than the 10.24 industry average. And in terms of non-GAAP forward P/E, the company's 14.44x compares with the 14.60 industry average. And its 1.05x forward Price/Sales is 11.1% higher than the 1.18x industry average.
POWR Ratings Reflect Uncertainty
LEG has an overall C rating, which translates to Neutral in our POWR Ratings system. The POWR Ratings are calculated by considering 118 distinct factors, with each factor weighted to an optimal degree.
Our proprietary rating system also evaluates each stock based on eight distinct categories. LEG has a D grade for Growth. Analysts' expectation that the stock's EPS will decline 3.9% in the current quarter is in sync with the grade.
In terms of Sentiment grade, the company has a C. Also, LEG has a Momentum grade of C, which is consistent with its price returns over the past month.
In addition to the grades I have highlighted, one can check out additional LEG ratings for Quality, Stability, and Value here. LEG is ranked #49 of 61 stocks in the B-rated Home Improvement & Goods industry.
While LEG witnessed 8% organic sales growth in the third quarter due to increased raw material selling prices, a significant fall in its volume and EBIT margin could hold back its growth as it continues to battle supply chain woes. Furthermore, rising costs driven by inflationary pressure could add more uncertainties to its path. Thus, we think investors should wait until the company better navigates the challenges.
How Does Leggett & Platt (LEG) Stack Up Against its Peers?
While LEG has an overall C (Neutral) rating in our proprietary rating system, one might want to check out its industry peers with A (Strong Buy) ratings: Acuity Brands, Inc. (AYI), Duluth Holdings Inc. (DLTH), and Masonite International Corporation (DOOR).
LEG shares were unchanged in premarket trading Monday. Year-to-date, LEG has declined -7.47%, versus a 27.55% rise in the benchmark S&P 500 index during the same period.
About the Author: Imon Ghosh
Imon is an investment analyst and journalist with an enthusiasm for financial research and writing. She began her career at Kantar IMRB, a leading market research and consumer consulting organization.
The post Is Leggett & Platt a Buy Under $40? appeared first on StockNews.com
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ALP RM Miro Series Reflectors are made of highly polished aluminum and feature a smooth rolled metal design, minimum reflectance of 95 percent and a 25 year warranty. The reflectors are corrosion resistant and formable. The smooth, unblemished surface of the Miro aluminum reflectors prevents light striations, acheives maximum efficiency from light fixtures, functions in hostile environments, and can be shaped for ultimate light control.


Every digital editor has been there.
Your job is to manage your brand's Instagram feed, but you got behind and are scrambling for content. The quality of the feed suffers, and engagement goes down. Before you know it, your feed looks so second class.
Panic? Nah. You don't go out like that.
We got you covered. Read on to learn how to ensure you always have beautiful, branded content that engages on Instagram.
Brands live and breathe Instagram. It's their life source, and is the top priority channel for building brand awareness, engaging fans, and converting new customers. A brand lives and dies by the quality of the content in its feed, and can't risk getting behind on its content schedule. Ask any social media editor how hard it is to stay on top of things.
Here are four ways to keep your feed game tight.
You have a great eye, and someone on your team probably does too. Make it a point to be active in taking photos and short videos that could work on your brand's feed. Take shots of the office, behind the scenes at shoots, at the design department, or even of your favorite brunch. Keep shooting, and you will be certain to have a bank of great content to mix into your feed.
Hope you have a 128GB, cuz that iPhone's gonna be bursting with delicious snaps.
One of the great things about Instagram is that it gives content creators (bloggers, cool kids, your fans) the ability to tag you in comments and photos. When they wear one of your products and tag you in a post, they're asking you to check them out, often hoping to be featured on your feed.
While not all user generated content is created equal, there are many diamonds in the rough that you can add to your editorial calendar. Sifting through hashtags is a poor use of time even for an intern, and Instagram does not provide a way to search photo tags or comment mentions.
Dash Hudson to save the day. We created a free monitoring tool to help surface the best content featuring your brand, by bringing you the highest quality photos you've been photo or comment tagged in.
Events and branded adventures are a great way to reward loyal fans, engage influencers, and capture incredible content. Whether it's a luxurious trip to BVI, a drive up the PCH, or exclusive event at your shop, these provide an opportunity to capture lots of high quality, organic, lifestyle photography that supports your brand.
Protip: add influencers to the mix to amplify the exposure of your adventure.
The best way to get high quality, well-composed content for your Instagram feed is to partner with influencers to produce it. The right influencer will create natural, organic content featuring your product, and share it with an audience of potential new customers. You get rights to the content, and you get exposure. Two wins. The cost of working with a team of high quality influencers will certainly be less than your last editorial photo shoot. This data also speaks for itself. ROI, baby.
There are some secrets as to how to do it right, and we can help.
There you have it. Four ways to create high quality, branded content to build a beautiful Instagram feed. It takes a bit of planning and commitment, but the impact on content quality, follower engagement, and ROI will be significant.
PS: If you dug this, come learn more about how Dash Hudson can help you create a killer Instagram feed, build your brand, and reach new customers.


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The inaugural Cinco K Mayo® will be held on Cinco De Mayo (5.5.19) at Jose's Blue Sombrero in Mount Pleasant, WI – Celebrate in style for this new and unique run in Southeast WI.
RUN FOR FREE! Raise over $100 in pledges and we will credit your registration up to $30. Download our pledge form here: http://www.5kevents.org/pledgeform.pdf .
Racine Youth Sports provides quality, structured youth sport activities to the children of Racine County. The developmental programs teach sports fundamentals, good sportsmanship, character, discipline, competitiveness, and teamwork in a positive, caring and safe environment. Participants have an equal opportunity to learn and compete while knowledgeable volunteers will promote the philosophies and principles of community and fair play.
Starting at Jose's Blue Sombrero through the Pike River Preserve in Mount Pleasant, WI and back to Jose's for some TEQUILLA!
The run starts promptly at 9:00 am. We recommend arriving early and giving yourself enough time to get your race packet and get to the start line. Runners should start in the front. Walkers toward the back. Anyone with a stroller will need to start in back.
Parking is available throughout Jose's parking lot and neighboring businesses. To help minimize traffic near the start/finish line, no vehicles will be able to enter or exit Jose's parking between 8:30 and 10:15 a.m. If you need to depart before 10:15 a.m. we suggest using one of the neighboring businesses to park.
All participants will receive a custom finishers medal.Top three male and female will be recognized as well as the top male and female in respective 5 year age groups.
If you wish to be timed, your chips will be issued to you with your race bibs. You must properlly wear the race bib on the front of your shirts and the timing chips on your shoes during the event to be scored. Race chips are disposable and do not need to be returned.


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Hundreds reach out to victims of domestic violence at JandJ
BREAK THE SILENCE: DVAC's team of volunteer knitters hope their tree jumper will encourage victims of domestic violence to seek support. Domestic Violence Action Centre
by Bianca Hrovat
Bianca Hrovat Journalist
THE hands of hundreds of men, women and children will reach out to victims of domestic violence during Jumpers and Jazz in July.
The Domestic Violence Action Centre created a tree jumper in the hope of shedding the stigma of domestic violence and creating connections between victims and support services.
The tree, constructed by around 10 volunteers, will feature the felted hands of people from all walks of life, from courthouse staff to children at childcare centres.
The public show of support is more important than ever as case workers report a noticeable increase in domestic violence incidents across Warwick.
DVAC service manager Kathleen Turley said staff were in Warwick on a fortnightly basis to support women through the court process.
"Sometimes people think it doesn't happen in their community because they don't necessarily see it or hear it but it happens everywhere in Australia," she said.
"We have to start a conversation about what may or may not be happening in the Warwick area.
"It's definitely prevalent."
The tree jumper, entitled "Where flowers bloom, so does hope", will provide women with a subtle way of seeking out help.
"One of the greatest challenges we have with public events is that they don't want to be seen talking to us," Ms Turley said.
"At Jumpers and Jazz everyone is going to be milling around and once they get to the tree it will be easy for them to take a brochure and move on."
The service manager said women often avoided seeking help due to feelings of shame or concerns about safety.
"The perpetrator may have a connection with a number of people so for a woman to disclose what's happening to her may impact her safety," Ms Turley said.
Victims of domestic violence who are inspired to contact DVAC can expect a judgment-free support zone.
"People can choose the sort of support they want and we don't pressure them into doing anything," Mrs Turley said.
"We will listen, give lots of different options and walk alongside them in their choices."
Though many women have come through DVAC and out the other side with established jobs and secure accommodation, Mrs Turley said staff at the centre considered every woman contacting their service to be a success story.
"It's a really positive opportunity to share stories and get support," she said.
If you, or someone you know, requires assistance phone DVAC on 4642 1354 (counselling during business hours) or for 24 hour support phone Womensline on 1800 811 811 or Mensline on 1800 600 636.
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