text:
\section{Introduction}

Coronal mass ejections (CMEs) are huge explosions of magnetized plasma from the Sun.
Their interplanetary counterparts, interplanetary coronal mass ejections (ICMEs), are
considered to be the main driver of geomagnetic storms \citep{Gonzalez:etal:1994}.
The major scientific objective of the \textit{Solar TErrestrial RElations Observatory}
(STEREO) mission \citep{Kaiser:etal:2008} launched in October 2006 is to better
understand the initiation and propagation of CMEs. A big advantage of the STEREO twin
spacecraft is that they allow a simultaneous observation of a CME from two different
perspectives. Quite a number of papers have been dedicated to the 3D reconstructions
of CMEs based on the coronagraph observations of the STEREO spacecraft.

Different reconstruction methods of coronagraph observations have
been used in the past. Among them are forward modeling, triangulation
method, polarisation ratio method. A review on these
methods can be found in, e.g., \citet{Mierla:etal:2010}.
\citet{Antunes:etal:2009} used a combination of forward and inverse
method to estimate the CME mass distribution.

In this paper, we are aiming to obtain the 3D morphology of a CME by using the
coronagraph observations from three viewpoints. Unlike forward modeling where
a restricted family of geometrical CME shapes is assumed beforehand, our
method allows any a-priori shape of a CME.
For tie-point approaches, the identification of corresponding structures from
different views is required but is often difficult to achieve. The method
described in the current work does not have this problem.
The polarisation ratio method utilises the polarising properties of the
Thomson scattering. In principle, only one view is required.
However, the
information returned is only a depth surface representative of the
scattering centres in the CME cloud along the line-of-sight. No information
about the depth distribution can be retrieved. Moreover, the resulting plane
bears the ambiguity of two symmetric solutions with respect to the plane of
sky. The combination of forward and inverse methods of \citet{Antunes:etal:2009}
also uses a forward modelling step essentially based on family of flux rope CME
models. In a second step, the flux rope 3D volume is then used as the
support for an inverse estimation of the density distribution of the CME.
The latter step, however, is heavily under constrained and multiple solutions
are possible.

Along with the very large variety of coronagraph reconstruction
techniques, 3D geometric reconstructions using heliospheric imagers have also
been developed by some authors, where a CME was treated as a complete volume
rather than a point source. For example, \citet{Lugaz:etal:2009} used a 3D
magneto-hydrodynamic code to disentangle observational from physical effects.
By comparing the simulation with the observations from coronagraph and
heliospheric images,
the 3D nature of two successive CMEs and their evolution in the inner heliosphere
were studied. \citet{Tappin:Howard:2009} compared their model of interplanetary
disturbances with heliospheric image data from the Solar Mass Ejection Imager.
By identifying the simulated ICME that best matched the observations, they
obtained the parameters that can describe ICME's 3D leading-edge structure,
orientation and kinematics.

The CME localisation and morphology in 3D yield information about the CME's
orientation, propagation direction, angular width in longitude and latitude
etc. and help to make reliable predictions about the arrival time
of a CME at Earth or other planets. Reversely, in-situ observations can
be combined with near-Sun 3D reconstructions to constrain the CME model
a-posteriori.
Such investigations aimed to study CME propagation properties in the
interplanetary space have been performed by some authors, e.g.,
\citet{Mostl:etal:2009, Byrne:etal:2010, Liu:etal:2010a, Liu:etal:2010b,
Rodriguez:etal:2011}. \citet{Rouillard:etal:2009} investigated a CME observed
between Sun and Venus using the STEREO, \textit{Venus Express} (VEX) and
MESSENGER data. They compared the (I)CME orientation obtained by white light
analysis with the in situ flux rope axis by MESSENGER and VEX. The CME
orientation in the STEREO/COR2 field of view (FOV) was derived by a fit of the
graduated cylindrical shell (GCS) model \citep{Thernisien:etal:2006,
Thernisien:etal:2009, Thernisien:2011}. Due to the limited separation angle at
the time of these observations, the GCS flux rope was only fitted to COR2 A.
Early work before the STEREO era devoted to the comparison of the orientation
of the source region neutral line, the CME cloud shape in coronagraph images
and the flux rope axis orientation from in situ measurements have been made by
\citet{Yurchyshyn:etal:2001, Cremades:Bothmer:2004, Yurchyshyn:2008}.

In this paper, we propose a new method for the reconstruction of the
CME cloud based on the back projection of the observed CME periphery in
multiple coronagraph images without any restriction by a predefined
class of CME shapes.
From the superposition of these back projections, we obtain a 3D volume which
must contain the CME cloud entirely. Reversely, the real CME cloud also must
fill this 3D volume in the sense that the cloud has to touch each wall
of the 3D volume somewhere. Based on these principles, we propose a scheme
to obtain an approximation to the real 3D CME cloud shape.
Since the problem of 3D reconstruction from 2D images is notoriously
under constrained, we have designed our scheme so as to incorporate
images from as many different view directions as possible. In the
application presented here, coronagraph data from three spacecraft
were used.

The paper is organised as follows:
In \S 2, the coronagraph observations from three vantage points, STEREO A \& B,
and SOHO are described.
Details of our reconstruction method are presented in \S 3.
In \S 4, we use the 3D morphology obtained from our reconstruction to
interpret in-situ magnetic field and plasma parameters observed during the
passage of the CME near Venus, Earth, and two STEREO spacecraft. The data we
consider were obtained by
the magnetometers (MAG) onboard VEX orbiting Venus, \textit{Advanced Composition
Explorer} (ACE) orbiting Earth, and from
the In-situ Measurements of Particles and CME Transients (IMPACT) and The Plasma and
Suprathermal Ion Composition (PLASTIC) telescopes onboard STEREO.
From a series of 3D reconstructions with time, we are able to follow the CME
morphological evolution. The height, speed evolution from the Sun to Venus
are also discussed.
The orientation of the filament in the source region, the orientation of the
CME major principle axes and the flux rope axis direction derived from VEX/MAG
data are compared.

\section{Observations and data reduction}

The CME we have investigated was observed on August 7, 2010 from three
perspectives by the white light coronagraphs
Large Angle Spectroscopic Coronagraph
(LASCO; \citet{Brueckner:etal:1995}) C2 and C3 onboard the \textit{Solar and
Heliospheric Observatory} (SOHO; \citet{Domingo:etal:1995}), COR1 and COR2 in the
the Sun Earth Connection Coronal and Heliospheric
Investigation (SECCHI; \citet{Howard:etal:2008}) instrument suite onboard STEREO.
LASCO C2 has a FOV from 2 to 6~R$_{\odot}$, C3 from 3.7 to
30~R$_{\odot}$. COR1 reaches a lower altitude with its FOV from 1.4 to
4~R$_{\odot}$, COR2 from 2.5 to 15~R$_{\odot}$.
On August 7, two STEREO spacecraft were separated by around 150 degrees.
The spatial positions of STEREO A and B, the planets and their orbits in the inner
solar system are presented in Figure~\ref{fig:HEE_posi} in the Heliocentric Earth
Ecliptic (HEE) coordinate system. Venus was located between STEREO B and the
Earth. The magnetometer onboard VEX \citep{Zhang:etal:2006} will be utilised to verify the CME
propagation direction and to determine the CME arrival time at Venus.

In Figure~\ref{fig:corAB_lasco} we present the time series of coronagraph
images of the CME event for the three viewpoints employed. All images were
processed by standard Solarsoft routines secchi\_prep and lasco\_prep.
COR1 and COR2 images from STEREO A are shown in the first row, COR
images from STEREO B are in the second row, and the C2 and C3 images
from LASCO are presented in the last row.
In each panel, the operated instrument and observational time are marked at
the bottom. The occulter of coronagraph is indicated as a black mask. As a size
reference, we also plot the solar limb as a white circle onto each panel.
Two different background subtraction methods have been applied here to
make the CME leading edge and its related shock more prominent.
For COR data, the respective pre-cme images were subtracted. For LASCO-C2, a
12-hour minimum image was created by taking the minimum brightness of each
pixel during the 12 hours centred around the CME's first appearance.
The dark area inside the CME in COR1 and COR2 indicates the position of a
preexisting helmet streamer which stayed more or less quasi-stationary during
the CME evolution.
The first appearance of the CME in COR1 A was at 18:15, in
COR1 B at 18:25 UT, and in C2 at 18:36 UT.

For this particular CME, we identified shock signatures in the white-light
observations. They appeared as a smooth front which outlined
the CME out-most envelope and was
associated, spatially and temporally, with streamer deflections
\citep{Ontiveros:Vourlidas:2009}. They are marked in column 5 in
Figure~\ref{fig:corAB_lasco} with two deflected streamers accompanied closely.
At lower altitudes as in column 2, the shock looked like a diffusive area
enclosing the CME cloud \citep{Gopalswamy:Yashiro:2011,Gopalswamy:etal:2012}. It is best seen
in the C2 image of column 2 where the CME periphery is
indicated by plus signs. The presence of a shock for this CME event is
confirmed by the type II radio burst at a height of about 1.36~R$_{\odot}$ (N.
Gopalswamy 2011, private communication).

The shock signature can presumably be linked to the coronal EIT waves
down to the FOV of EUVI \citep{Wuelser:etal:2004} onboard STEREO \ and AIA
\citep{Lemen:etal:2011} onboard SDO (\textit{Solar Dynamics Observatory}),
which are 1.7 and 1.3 solar radii, respectively. In panel (a), (b), and (c) of
Figure~\ref{fig:cme_ini}, we present the dimming and the wave front
in the running difference images observed by EUVI B, AIA, and EUVI A. An
animation of the high-cadence AIA observations is available in the online
journal where the coronal wave signature can be seen more prominently. The wave
signatures observed above the limb were well connected to the wave signatures
observed against the solar disk. EUVI A
provided a better view of the wave dome. Inside the dome, the erupted
prominence was visible in panel (f). The prominence in 30.4 nm is colored
in red, while the wave front is colored in light blue.  When the CME
entered the COR 1 FOV (panel (e)), the CME periphery and shock
front are delineated by plus signs and asterisk signs,
respectively. In the same panel, the CME associated streamer belt
is also shown. Details of the shock/EIT wave analysis is
beyond the scope of this paper and will be pursued in a
separate paper. Similar wave behavior and related quantative
analyses can be found in, e.g., \citet{Veronig:etal:2010}.

The subtraction of the pre-CME image somehow removed part of
the internal structure of the CME. To make the internal structures visible,
for COR 1 images we applied the 12-hour minimum image as well. The resulting
images are shown in panel (d) of Figure~\ref{fig:cme_ini}. The CME periphery
we used for 3D reconstruction is
indicated as black asterisk signs. We tried to exclude as well the sheath between
the shock front and the CME which manifested as a diffusive region there.
Red plus signs represent the outer boundary of the CME cavity and the area inside
green signs indicates the core region. For this CME, we found that
its internal structure is a little bit complicated. In the cavity, it seems that
a bright line feature appeared.
If we regard the CME flux rope as the cavity and the prominence attached below
\citep{Chen:1996}, the area inside the red signs is mainly the CME flux rope
and possibly some material following it. Except the unknown part hidden behind the
occulter, we found that the CME flux rope occupied most of the area surrounded
by the black signs, which we used for the 3D reconstructions.

In order to locate the CME source region, we have checked EUV images at
various wavelengths taken by the EUVI instrument
onboard STEREO and by the AIA telescope onboard the
SDO spacecraft. At the time of the CME
launch, a M1.0 class flare occurred in active region AR~11093 located at
N12E31 as viewed from Earth on August 7. According to GOES light curves, the
flare started around 17:55 and peaked at 18:24. Magnetograms from HMI
(Helioseismic and Magnetic Imager, \citet{Scherrer:etal:2011}) were used to
determine the orientation of the magnetic polarity inversion line in the CME
source region.

\section{3D reconstruction method}

\subsection{3D reconstruction and smoothing}

In the traditional stereoscopic technique, two corresponding points
from an image pair are back projected along the respective line-of-sight to
obtain their 3D coordinates
\citep{Inhester:2006,Feng:etal:2007a,Feng:etal:2009, Liewer:etal:2009,
Liewer:etal:2011}. \citet{deKoning:etal:2009} geometrically reconstructed
the CME location plane by plane from two viewpoints. The authors selected
two points on the CME boundary in each image and back-projected to the Sun
totally four points which lie in the same plane. Their back-projections
formed a quadrilateral in that specified plane where the CME is ideally
localised. Later, \citet{deKoning:Pizzo:2011} included the geometric localisation
method into the polarimetric technique to remove the ambiguity inherent
in this technique.

The idea of our reconstruction method employs the inverse
approach of the traditional stereoscopic technique. In this newly developed
method, we forward project a point in the 3D space onto each coronagraph
image. If the three projections are all located inside the respective CME
periphery observed in each image, this 3D point is considered as a point
inside a 3D volume which must contain the 3D CME cloud entirely.
On the other hand, for the CME surface to be consistent with the observed
peripheries, it must be close enough to the boundary of the
reconstructed 3D volume so that their projections onto the coronagraph
images coincide.

In a first step, we identify the CME periphery in each coronagraph image.
At the moment, it is done by tie-pointing the CME leading edge in each
image. The tie-points are then interpolated by a parametric cubic spline
to obtain a smooth periphery curve.
Examples of periphery tie-points are shown in column 2 and
6 of Figure~\ref{fig:corAB_lasco}. Since we do not know how the CME
continues behind the occulter, we simply extrapolate the ends of the
periphery curve from the occulter edge radially to the Sun's surface.
The result of this step is saved as binary masks $M_i(x_{p,i},y_{p,i})$
for each image $i=A,L,B$ taken by STEREO A, LASCO and STEREO B, respectively.
We set $M_i$ to unity at image pixels
$(x_{p,i},y_{p,i})$ inside the periphery curve and to zero outside.
Note that the LASCO images were not always recorded exactly simultaneously
to those from STEREO. In these cases, the CME periphery curves from
two neighbouring frames in time from LASCO were interpolated to the time
of the STEREO observations.

As the next step, we select a regular 3D mesh of the space around the Sun. In
our method, the distance of grid points is chosen adaptively depending on the
projected CME size in the images. Since we are considering a time evolution
problem, all calculations in this work are performed in a Cartesian Carrington
coordinate system.
For each 3D grid point $\mathbf{r}=[x,y,z]$ we obtain its projection
$\mathbf{r}_{p,i}$ onto image $i$ by \citet{Feng:etal:2007b}.
\begin{equation}
\mathbf{r}_{p,i}=A_i^T\mathbf{r}
\label{equ:project}
\end{equation}
where $A_i$ is the the matrix of the coordinate transform
\[
A_i=
\left[ {\begin{array}{ccc}
 -\sin L_i & -\cos L_i\sin B_i \\
  \cos L_i & -\sin L_i\sin B_i \\
  0        &  \cos B_i         \\
 \end{array} } \right]
\]
and $L_i$ and $B_i$ are the longitude and latitude of spacecraft $i$ in the
Carrington coordinate system. After projecting a 3D point $\mathbf{r}$ onto
all three coronagraph masks $M_i$, we set a 3D mask $M_{3D}$ according to
\begin{equation}
M_{3D}(\mathbf{r})=\begin{cases}
   1 \quad\text{if}\;M_i(\mathbf{r}_{p,i})=1\;\text{for all}\;i=A,L,B\\
   0 \quad\text{if}\;M_i(\mathbf{r}_{p,i})=0\;\text{for one or more}\;i
\end{cases}
\end{equation}
This process is repeated for all 3D points until the 3D mask $M_{3D}$ is
completely determined. This mask then defines the embedding 3D volume
containing the CME cloud.

As an example of the reconstructed 3D mask we show a horizontal cut of
$M_{3D}$ which yields the polygon in Figure~\ref{fig:bezier}. The mask area is
marked by plus signs at the respective grid points. The region defined by mask
$M_{3D}$ may include areas which do not belong to the true CME area but are
yet covered but the projections of the 2D image masks. Assuming the real CME
surface is smooth, these areas are probably confined to the vicinity of the
vertices of the polygon from $M_{3D}$. These vertices occur naturally where
the boundaries of the back projected 2D masks intersect. From three images
there are up to six vertices possible in every horizontal plane intersecting
$M_{3D}$. In Figure~\ref{fig:bezier}, these vertices are marked as diamonds.

In a final step, we smooth the corners of $M_{3D}$. For each horizontal plane,
we find the centres on the faces of the 3D mask between each neighbouring pair
of vertices. In Figure~\ref{fig:bezier}, these centres are marked as stars. For
each vertex we then define a quadratic B\'{e}zier spline
\begin{equation}
\mathbf{B_i}(t)=(1-t)^2\mathbf{P_{i-1}}+2(1-t)t\mathbf{P_i}+t^2\mathbf{P_{i+1}}
 ,\quad t\in[0,1]
\label{equ:bezier}
\end{equation}
from the three control nodes $P_{i-1}$, $P_i$ and $P_{i+1}$. The central
$P_i$ is the vertex position and $P_{i\pm1}$ are located at the face centres
to either side to the vertex. This choice of the spline curve insures that
the boundary formed by the combination of all spline curves is continuous
and smooth as demonstrated by the example in Figure~\ref{fig:bezier}.
This new boundary is finally adapted as the approximation to the CME shape
in each horizontal plane.

Similar techniques were used in earlier papers. \citet{Byrne:etal:2010} fitted
an ellipse to a quadrilateral which was derived from two viewpoints. However,
our B\'{e}zier curve fitting has more flexibility and is readily adapted to
include more than two view directions.
Additional view directions provide more constraints to the 3D CME localisation.
However, we have to admit that as the control nodes on the face centres are
selected somewhat arbitrarily, there is still some uncertainty about the
real CME shape. From our procedure we obtain the surface with the
least curvature compatible with the observations.

This fitting process described above is performed for each horizontal plane.
In the end, a smoothed surface of the CME cloud is obtained. One example of
such reconstruction is shown in Figure~\ref{fig:prin_axis_eg} and is
represented by red curves. We have to mention that since the CME structure
below the occulter is unknown, the CME cloud in the region inside the
occulter radius from the Sun's centre is not plotted.

\subsection{Calculation of the geometric centre and principle axes}

Since a determination of the density distribution in the CME cloud
is a highly ill-posed problem and can not be done reliably from only
three view directions without further constraints, we take the CME
shape as the basis for a further analysis.
We therefore neglect the internal structure of the CME in the analysis
below and only characterize the shape of the cloud and its morphological
evolution. Hence the centre of the cloud may not be its centre of gravity,
but the geometric centre which is still a significant
quantity to characterise the position and motion of the CME cloud.

Natural characteristics of an amorphous volume are its geometric centre
(GC), its three principle axes and their eigenvalues. The geometric centre
$\mathbf{r_{gc}}$ of the CME cloud can be obtained from
\begin{equation}
\mathbf{r_{gc}}=\frac{\sum_\mathbf{r} V(\mathbf{r})\mathbf{r}}
{\sum_\mathbf{r}V(\mathbf{r})}
\label{equ:cgrav}
\end{equation}
where $V(\mathbf{r})$ is unity inside the CME cloud and zero elsewhere.
The principle axes and their eigenvalues are found from a diagonalisation
of matrix
\begin{equation}
\frac{\sum_\mathbf{r}V(\mathbf{r})(\mathbf{r}-\mathbf{r_{gc}})
     (\mathbf{r}-\mathbf{r_{gc}})^{T}}
     {\sum_\mathbf{r}V(\mathbf{r})}
\end{equation}
These integrations are straight forwardly performed on the 3D grid chosen
to generate the mask $M_{3D}$. Grid cells intersected by the boundary of
$V(\mathbf{r})$ are weighted according to their overlap with $V(\mathbf{r})$.

In Figure~\ref{fig:prin_axis_eg}, we plot the directions of three eigenvectors
calculated from the matrix diagonalisation for the CME cloud at 21:24. The
thickness of three principle axes is proportional to the magnitude of
eigenvalues. All three eigenvectors are centred at CME's geometric centre.
We name minor, intermediate and major axis, respectively, according
to the order of their eigenvalues.

\section{Results}

Based on the reconstructed 3D surface of the CME cloud, further analyses can
be made. A straight forward application is to identify the longitude and
latitude of the CME cloud and its spatial extension in 3D. This information
can assist to interpret in-situ measurements. From a time series of the 3D
cloud, the CME's morphological evolution and propagation
properties can be derived.

\subsection{Interpretation of the in situ data}

From the space weather point of view, the longitude and latitude
position, the angular width of the CME cloud are very crucial to determine
whether or not a CME can interact with a planet's magnetosphere or
a spacecraft.

Figure~\ref{fig:topview} provides a view from a vantage point above the
solar north pole in which the localisation of CME relative to the Sun,
Venus and two STEREO spacecraft are indicated. The CME initiated on August 7 was
propagating closely towards Venus. In Figure~\ref{fig:vex}
we present the magnetic field measurement by the Magnetometer onboard
Venus Express (VEX/MAG) from August 9 to 12. From top to bottom, we
plot the total magnetic strength
and three magnetic field components in the Radial-Tangential-Normal (RTN)
coordinate frame. Here, vector $R$ is the unit vector from Sun to the
spacecraft , $T$ is the unit vector in the direction of the cross product of
$R$ and solar rotational axis, and $N$ completes the right-handed triad. VEX
has an elliptical polar orbit with a 24-hour period, and stays in the Venusian
magnetosheath and magnetosphere from 07:00 to 10:20 UT for each orbit. MAG
continuously operates, but we block the data from 07:00 to 10:20 UT to focus
on the solar wind structure.

On August 10, from about 04:00 UT MAG detected a sudden
discontinuous increase in the magnetic field strength and the abrupt changes
in the field direction. It is likely the shock and sheath signature preceding
an ICME. Further verification requires also a sudden increase in flow speed,
density and thermal speed. Unfortunately, plasma measurements by VEX was
not available for the solar wind structure. The spacecraft enters the
Venusian ionosphere when plasma measurements are made. From 11:00 UT on the
same day, the magnetic field strength was enhanced and smooth rotations of
the field were found. It implies the appearance of a magnetic cloud. Due to
the lack of plasma measurements, a further proof of the lower proton
temperature is not available in Figure~\ref{fig:topview}.

The magnetic field and plasma measurements in Figure~\ref{fig:insituB} taken
from the IMPACT and PLASTIC particle spectrometers onboard STEREO B only show the
signature of a shock which appeared around 10:00 UT on August 11. From top to
bottom, we plot the magnetic field in RTN coordinates and its total strength,
the proton density, the bulk speed and the proton temperature.
We did not see any clear ICME at STEREO B following the shock. This observation
can be explained by checking the CME localisation relative to the line
connecting the Sun and STEREO B in Figure~\ref{fig:topview}.
The flank of the reconstructed CME cloud just touches this connection line
which is an evidence that the cloud did not pass STEREO B. However, since the shock
has a larger spatial extension than the cloud, it was still observed at the
spacecraft. The projected shape of the CME on the solar
equatorial plane indicated that the CME was mainly directed to VEX and STEREO B.
Unfortunately, we do not have direct observations of the shock on the
equatorial plane, we speculate that the in-situ shock signature might be more prominent
in the VEX and STEREO B observations. We did not see any signature of an ICME
and/or a shock in the ACE data observed at L1 point.

\subsection{Morphological evolution of the 3D cloud}

By following the variation of the calculated eigenvalues and eigenvectors, we
can deduce the CME's morphological evolution. In Table~\ref{tab:eigen}, the
ratio of eigenvalues of the major to the minor axis, and of the intermediate
to the minor axis are listed. The related uncertainties are propagated from
the 2D CME tracing uncertainties.
In the first column, the average distance between the traced CME peripheries and
its standard deviation are presented. Here the 2D uncertainty is derived by
repeating the tracing process for ten times.
It can be seen that the major morphological differences occurred during the
first three time instances.
After 20:08 UT, the shape appears to have remained stable. This trend can also
been seen from the orientation of principle axes in
Figure~\ref{fig:prin_evol}.

We have to admit that our reconstruction is subject to another uncertainty.
From the coronagraph observations we can only observe the part of CME outside
of the occulter. This produces a larger uncertainty on the reconstructed CME
shape in the early phase of propagation when an unnegligible part of CME was
still below the occulter.
Therefore, the orientation of the reconstructed CME cloud at the earliest
time in Figure~\ref{fig:prin_evol} might have relatively big error bars.

In panel (a) of Figure~\ref{fig:prin_evol}, the intermediate principle axis at
four different time instances is shown from viewpoint of STEREO A. The black
sphere represents the Sun, the red sphere represents STEREO A. The green dots
are the geometric centre at different times. And the green line is the
linear interpolation of these green dots indicating the CME propagation
direction.
The projected CME cloud at 18:48 UT and 21:24 UT is presented as well in red
and blue in panel (a), respectively. We find that the orientation along
which the CME is most extended as seen in COR A is more or less consistent with
the intermediate axis, not with the major axis. It implies that for this CME, the
most elongated direction in 3D is not lying in the projected COR A image
plane.

The evolution of the intermediate axis shows big changes in orientation from
18:48 UT to 20:39 UT. This shape change is also evident in COR A observations.
In the early phase of the propagation, the northern part was moving ahead of
the southern part. The reason is that the northern part of the filament
related to this CME erupted first \citep{Reddy:etal:2011}. Later on, the
southern part of the CME entered the fast solar wind region and was probably
accelerated. The interaction of the CME with the fast and slow solar wind
components likely produced a heart-like shape. The slow solar wind
appears to originate from a region that is known as the streamer belt, which
was around the solar equatorial plane as can be seen in panel (e) of
Figure~\ref{fig:cme_ini}. Because the CME had a speed (see \S 4.4) greater
than the slow solar wind, say typically about 400 km~$s^{-1}$, it became
significantly decelerated near the streamer belt; whereas the part of CME
in higher latitudes might even be accelerated, if the ambient fast solar wind
had a higher speed. Varying conditions at different latitudes
likely caused the distortion of the CME structure.
It can also be seen in panel (a) that the
propagation of the CME geometric centre points more or less to the dip of the
concave inward bulge of the CME shape which marks the position of the
streamer belt.

Panel (b) shows the major axis projected onto the solar equatorial plane.
The thin orange solid line is the direction perpendicular to the CME
propagation. We find that the orientation of the major axis does not show much
variation during the CME evolution. Interestingly, it is not perpendicular to the
propagation direction. The asymmetry with respect to the propagation direction
probably reflects a west-east asymmetry of the filament eruption.

Panel (c) presents the evolution of the major axis as seen along the
propagation direction. Again we find an almost constant orientation during the
later phase of the CME evolution. Our analysis indicates a rotation of the
major axis in the early stage from 18:48 UT to 19:54 UT. However, this rotation
might also be due to the uncertainty of the CME shape at 18:48 UT introduced by
the part of the CME still hidden behind the occulter. A comparison of the
orientation of the CME with the related filament and in-situ ICME will be
discussed in \S 4.3.

The last panel in Figure~\ref{fig:prin_evol} shows the intermediate and the
major axes together with the projected CME cloud as seen from the perspective
perpendicular to the CME propagation at 18:48 UT and 21:24 UT. The major axis
at 19:54 UT and 20:39 UT from
this perspective are plotted as well. It is clear that the
shape has changed significantly from 18:48 UT to 21:24 UT. Again, the most obvious
change is during the early phase of the evolution.

\subsection{The source region and orientation comparison}

Extrapolating of the CME geometric centre propagation direction backwards to
the solar surface, we arrive at a location very close to AR 11093. Considering
the error bar of the 3D reconstructions especially at the early phase of the
propagation, the active region may be regarded as the possible
source region. The extrapolation of the geometric centre is quite helpful
for the identification of a CME's source region, especially
around the solar activity maximum when there are multiple active regions and
more frequent activities.

Reddy et al. (2011) and Srivastava et al. (2011) made detailed analyses of AR
11093. They found that it was the rising of a filament that led to a M 1.0
class flare and the CME on August 7, 2010. Here we present some
complementary investigations of the source region. In Figure~\ref{fig:sourcer}
are AIA and HMI observations. The upper panel shows the EUV image
at 304~\AA~right before the flare with HMI magnetogram contours overplotted.
The lower panel shows the post-flare arcades observed at 171~\AA~by AIA well
after the CME release.

From GOES observations we find that the flare started around 17:55 UT and peaked
at 18:24 UT. The filament marked 1 in Figure~\ref{fig:sourcer}, upper panel,
rose before the flare which is also indicated by the deviation of this
filament to the magnetic polarity inversion line (PIL). As filament 1 is
relatively high, the projected filament is, due to the projection effect, not
lying along the PIL. However, filament 2 seems to be consistent with the PIL.
Its disappearance is probably related to the heating by the flare.

The orientation of the PIL in the active region approximated by filament 2 can
be compared with the orientation of the major principle axis calculated from
the 3D CME cloud and the flux rope orientation deduced from the VEX/MAG data.
We note that the orientation derived from the VEX data only involves
the flux rope component in a CME, while the major axis of the reconstructed
3D CME is related to the leading edge, flux rope and possibly some material following
it. In Section 2 we found that the CME flux rope in the coronagraph image
occupied most of the area which we used for the 3D reconstructions, the major
axis is used as a first approximation of the orientation of the 3D CME
flux rope.

The filament is curved as seen from Figure~\ref{fig:sourcer}, we can
only make a rough comparison. The general orientation of the filament lies in
the direction from northeast to southwest which is consistent with the major
axis indicated in panel (c) of Figure~\ref{fig:prin_evol}. The orientation of
the flux rope observed by VEX was computed by the Minimal Variance Analysis
(MVA) method. It has a direction of (0.96, 0.01, -0.29) in RTN coordinate
system which means that the detected flux rope is mainly in the radial
direction. Compared with the flux rope orientation in the remote-sensing data,
there is a big difference. From the top view of the
reconstructed 3D CME in Figure~\ref{fig:topview}, it seems realistic that only
the leg of the flux rope structure passed through VEX. In
consequence, the orientation measured by MAG indicates a nearly radial direction.
If a spacecraft traveled through different parts of the magnetic cloud, the flux rope
orientation seen by the spacecraft may vary significantly. A diagram depicting
the possible VEX spacecraft path in the magnetic flux rope is shown in
Figure~\ref{fig:mc_ske}. However, if the spacecraft went through the flux
rope along the green path, we might arrive at a flux rope axis almost perpendicular
to the green direction.

\subsection{Propagation direction, height, and speed evolution }

In Figure~\ref{fig:lonlat_evo}, the trajectory of the CME
geometric centre is plotted. The figure shows its distance from the Sun and
its longitude and latitude. Near the Sun, the geometric centre has an
average speed near around 512 $\mathrm{km~s}^{-1}$.
The averaged longitude and latitude in the Carrington coordinates are -12.8
and -6.18 degrees, respectively. The CME was propagating roughly in the radial
direction. However, the latitude decreases from the source region at around 12
degrees in the northern hemisphere to -9 degrees in the southern hemisphere
at a distance of about 10 solar radii.
Similar deflections of a CME have been reported by
\citet{Cremades:Bothmer:2004} and other authors. CMEs which are launched
inside the solar activity belts at a time before the solar maximum and which
possess a total plasma and magnetic pressure less than the ambient solar wind,
are often deflected to the latitude where the slow solar wind resides.

After deriving the 3D localisation of the CME cloud, we also localise the part
of the CME leading edge around the solar equatorial plane directed to Venus.
In Figure~ \ref{fig:ht_vt}, the corresponding height-time (HT) plot is
presented in the left panel. The last point in the HT diagram is derived from
VEX data. It corresponds to the arrival of the ICME at Venus at around 11:00 UT on
August 10. The
$x$ axis is in units of hours starting from the beginning of August. On the
right side of Figure~\ref{fig:ht_vt}, the speed is calculated from the HT
plot with an exponential fit. The fit is constrained by HT data on the left.
The VEX data point was included such that the respective travel time of the
speed agrees with the distance to Venus.
We conclude from the low asymptotic speed of about 430~$\mathrm{km~s}^{-1}$
that the CME was embedded in the slow solar wind which severely decelerated
the CME.

\section{Conclusions and discussions}

We have developed a new method to obtain the 3D shape of a CME cloud without
assuming a predefined family of shape functions. We applied our method to a
CME which erupted on August 7, 2010. The geometric centre, three principle
axes and the corresponding scale along them were derived and their evolution
with time is presented. We could observe the evolution of the CME shape for
approximately 3 hours. We find that a significant deformation occurred during
the first two hours. During the last hour of observation, the shape evolution
was more limited and continued almost self-similarly. We attribute the change
of the CME morphology during the first two hours to its interaction with the
ambient solar wind. The projected CME major axes are found not
perpendicular to the propagation direction. It is probably due to
the east-west asymmetry of the CME related filament eruption.

The determination of the CME shape is helpful to interpret the in situ
observations by VEX/MAG, STEREO A \& B/IMPACT, STEREO A \& B/PLASTIC and ACE.
VEX detected a magnetic cloud following the preceding shock, STEREO B only saw
the shock. This is supported by our reconstruction which, if extrapolated out
to 1 AU, predicts that the CME just missed the location of STEREO B. For ACE,
the shock had probably dissolved into the background solar wind before it
arrived at the Earth. Therefore, ACE did not detect any shock signature.

By extrapolating the CME geometric centre propagation direction backwards to
the solar surface, we find that the source region of this CME is likely the
active region AR 11093 located at N12E31 in which a M1.0 class flare occurred
about 40 min before the CME became visible in the STEREO coronagraphs.
The rise of the destabilised filament led to CME eruption. The
orientation of the polarity inversion line in AR 11093 is in general
consistent with the major principle axes of the CME shape we have obtained
from its reconstructed shape.
However, it is not consistent with the flux rope axis deduced from the VEX
data with the MVA method. According to the reconstructed CME localisation in
the equatorial plane, it is very probable that only the leg of the CME flux
rope passed the VEX spacecraft. Indeed, the flux rope observed showed a
strong inclination in the radial direction.

A comparison of the latitude of the source region with the latitude of
geometric centre of the reconstructed 3D CME implies there
is a southward component of
its motion. If the plasma pressure and magnetic pressure in the CME is less
than that of the background solar wind, the CME is often deflected away from
the coronal hole where the fast solar wind dominates.

Combining the remote-sensing measurement and the in situ data from VEX, we
derive the 3D distance and speed evolution of the CME motion from Sun to
Venus. The CME speed decreases from 900 $\mathrm{km~s}^{-1}$ at one hour
after its initiation to 430 $\mathrm{km~s}^{-1}$. Probably
the CME speed was finally adjusted to the ambient solar wind flow.

\citet{Temmer:etal:2011} investigated at which heliospheric distance the drag
force starts to prevail over the driving magnetic force so that the speed of
the ICME gets finally adjusted to the speed of the ambient solar wind. They
analysed the observations of different CMEs and found that this heliospheric
distance varies considerably from below 30 $R_\odot$ to beyond 1 AU.
Theoretical and observational work on the driving and drag
forces during the CME evolution and propagation from the Sun to the
interplanetary medium can also be found in \citet{Chen:1996},
\citet{Manoharan:etal:2001}, \citet{Tappin:2006} and \citet{Howard:etal:2007}.
For the
CME we have analysed, we estimate that this distance at which the CME speed
becomes adjusted to the solar wind speed is beyond the FOV of COR2. Therefore,
to derive a reliable speed profile, eventually to make an accurate
prediction of the CME transit time on Earth or other planets, at least
Heliospheric Imager I (HI 1) in the SECCHI instrument package has to be
included for the investigated CME. In the near future, we will extend the mask
fitting method to HI observations.

A precise prediction of the CME travel time also depends on the accuracy of
the reconstruction method. Comparison of our mask fitting method and other 3D
reconstruction methods, for example, GCS forward modeling, polarisation ratio,
local correlation track combined with tie-pointing, geometrical localization,etc.,
will be presented in another paper. For this particular CME associated
with a complicated polarity inversion line, the forward modeling of the CME by
a single flux rope model will probably be not very successful owing to the odd
shape of the CME. A fit with two flux ropes might give better results. A
shortcoming of our mask fitting method is that the internal structure of the
CME is not included. We are planning to extend our shape reconstruction method
by a tomographic approach to determine a constrained density distribution
model within the 3D CME cloud.

\acknowledgements

We thank CDAweb for making the STEREO/IMPACT, STEREO/PLASTIC data available.
Thanks Marilena Mierla for many discussions on this work during her visit in the Max-
Planck-Institut for Solar System Research.
STEREO is a project of NASA. The SECCHI data used here were produced by an
international consortium of the Naval Research Laboratory (USA),
Lockheed Martin Solar and Astrophysics Lab (USA), NASA Goddard Space
Flight Center (USA), Rutherford Appleton Laboratory (UK), University of
Birmingham (UK), Max-Planck-Institut for Solar System Research (Germany),
Centre Spatiale de Li\`ege (Belgium), Institut d'Optique Th\'eorique et
Applique\'e (France), Institut d'Astrophysique Spatiale (France).
LF and WQG are supported by grants 10833607, 11003047 and 11078025
from NSFC and 2011CB811402 from MSTC.
The contribution of BI benefitted from support of the German Space
Agency DLR and the German ministry of economy and technology
under contract 50 OC 0904.

redpajama_set_name: RedPajamaArXiv


text:
Black-and-white photographs (26)
Color transparencies (12)
Gigabytes (12)
Color photographs (10)
Diaries (10)
Motion pictures (visual works) (10)
Black-and-white negatives (8)
Lantern slides (7)
Black-and-white transparencies (6)
Painters (17)
Art, Modern (14)
Museum exhibits (12)
Art museums (10)
Sculptors (8)
Museum curators (6)
Museum directors (6)
Printmakers (6)
Muralists (5)
Art historians (4)
Artists' studios (4)
Historical museums (4)
Women painters (4)
Hartley, Marsden (4)
Metropolitan Museum of Art (New York, N.Y.) (4)
Phillips, Duncan (4)
Tworkov, Jack (4)
Harvard University (3)
Henri, Robert (3)
Osborn, Robert Chesley (3)
Ray, Man (3)
Stella, Joseph (3)
Stieglitz, Alfred (3)
Storrs, John Henry Bradley (3)
Zabriskie Gallery (3)
American Artists' Congress (2)
Acadians (1)
Africans (1)
Afro-Brazilians (1)
Anishinaabe (Chippewa/Ojibwa) (1)
Basques (1)
Brazilians (1)
Dakota (Eastern Sioux) (1)
Jews (1)
Latinos (1)
Amsterdam (Netherlands) (1)
Anuradhapura (Sri Lanka) (1)
Breeze Hill (Harrisburg, Pennsylvania) (1)
Cincinnati (Ohio) (1)
Corinth (Miss.) (1)
DeKalb (Ill.) (1)
Detroit (Mich.) (1)
Disneyland (California) (1)
Smithsonian Institution Archives (34)
Query: Sydney International Exhibition (Sydney, Australia: 1879)
Exhibition Records
Hirshhorn Museum and Sculpture Garden. Department of Painting and Sculpture
1968-1993, with related records from 1956
66 cu. ft. (66 record storage boxes)
Record Unit 481
These records document the planning, development, and installation of exhibitions by the Department of Painting and Sculpture, Hirshhorn Museum and Sculpture Garden (HMSG). Included are biographical and bibliographical research files on artists; correspondence with museums, galleries, and artists concerning loan of artwork; loan reports; shipment records; installation notes and photographs …
in Record Unit 481 for Sydney International Exhibition (Sydney, Australia: 1879)
Curatorial Records
National Museum of American History. Division of Community Life
6 cu. ft. (6 record storage boxes)
Accession 06-164
This accession consists of the curatorial records of Carl H. Scheele during his tenure as Associate Curator in Charge and Curator in the Division of Postal History, 1964-1977; Curator in the Division of Community Life, 1978-1987; and as Curator Emeritus, 1987-1989. Materials primarily include correspondence, memoranda, and notes documenting professional activities, collections development …
in Accession 06-164 for Sydney International Exhibition (Sydney, Australia: 1879)
Downtown Gallery records
Downtown Gallery
109.56 Linear feet
AAA.downgall
The records of the Downtown Gallery date from 1824 to 1974 (bulk 1926-1969) and measure 109.56 linear feet. The records present a comprehensive portrait of a significant commercial gallery that operated as a successful business for more than forty years, representing major contemporary American artists and engendering appreciation for early American folk art. There is an unprocessed addition to this collection dating circa 1970 of a single financial/legal document.
in AAA.downgall for Sydney International Exhibition (Sydney, Australia: 1879)
Institute of Contemporary Arts records
Institute of Contemporary Arts (Washington, D.C.)
1927-circa 1985
AAA.instcona
The records of the Washington, D.C. arts and educational organization, Institute of Contemporary Arts, measure 36 linear feet and date from 1927-circa 1985, with the bulk of the material spanning the organization's active years, 1947-1967. The collection documents the arts and cultural programming organized by the ICA through correspondence, artists' files, program and exhibition files, administrative and financial records, printed materials and photographs. Also found are administrative, student, and teacher records of the ICA school; records of the Fine Arts Committee of the People-to-People Project; and some personal papers of the ICA's founder, Robert Richman.
in AAA.instcona for Sydney International Exhibition (Sydney, Australia: 1879)
Department of Anthropology records
National Museum of Natural History (U.S.). Department of Anthropology
Smithsonian Institution. Department of Anthropology
Smithsonian Institution. United States National Museum. Department of Anthropology
1840s-circa 2015
330.25 Linear feet (519 boxes)
NAA.XXXX.0311
The Department of Anthropology records contain administrative and research materials produced by the department and its members from the time of the Smithsonian Institution's foundation until today.
in NAA.XXXX.0311 for Sydney International Exhibition (Sydney, Australia: 1879)
National Museum of American History. National Numismatic Collection
26.91 cu. ft. (26 record storage boxes) (1 tall document box) (3 oversize folders)
This record unit consists of correspondence and memoranda pertaining to publications, exhibitions, acquisitions, numismatic conferences in foreign countries, and materials on loan; annual reports of the Division of Numismatics; budgetary files; American Numismatic Association convention information; exhibition scripts for the Hall of Monetary History and Medallic Art; policies regarding United …
Garry Knox Bennett papers
Bennett, Garry Knox, 1934-
AAA.benngarr
The papers of woodworker, sculptor, and furniture designer Garry Knox Bennett measure 12.4 linear feet and date from 1917 to 2017 with the bulk of the material dating from 1960 to 2017. The collection documents the artist's life and career through biographical materials, correspondence with family and friends including other artists, exhibition files, professional files, financial and legal records, and printed material and scrapbooks recording his exhibition history and more, including photographs from his youth.
in AAA.benngarr for Sydney International Exhibition (Sydney, Australia: 1879)
in AAA.breumarc for Sydney International Exhibition (Sydney, Australia: 1879)
Frank Perls papers and Frank Perls Gallery records
Frank Perls Gallery
AAA.perlfran
The Frank Perls papers and Frank Perls Gallery records measure 23.8 linear feet and date from 1920-1983, with the bulk dating from 1949-1975. Personal papers include writings, military records, appointment calendars, and photographs. Gallery records date from its opening in 1939 until its closure in 1981 and consist of financial, sales, and legal records; exhibition files; exhibition catalogs and announcements; subject files that contain a variety of correspondence with artists, dealers, galleries, museums, and friends and family, as well as reference materials and photographs; and scrapbooks.
in AAA.perlfran for Sydney International Exhibition (Sydney, Australia: 1879)
Kraushaar Galleries records
Kraushaar Galleries
0.181 Gigabytes
AAA.kraugall
The records of New York City Kraushaar Galleries measure 106.3 linear feet and 0.181 GB and date from 1877 to 2006. Three-fourths of the collection documents the gallery's handling of contemporary American paintings, drawings, and sculpture through correspondence with artists, private collectors, museums, galleries, and other art institutions, interspersed with scattered exhibition catalogs and other materials. Also included are John F. Kraushaar's estate records; artists' files; financial ledgers documenting sales and gallery transactions; consignment and loan records; photographs of artwork; sketchbooks and drawings by James Penney, Louis Bouché, and others; and two scrapbooks. There is a 6.0 linear foot unprocessed addition to this collection donated in 2022 that includes correspondence with artists, galleries, organizations and individuals regarding works of art, filed alphabetically by year. Materials date from circa 1959-1999, with the bulk from 1990-1999.
in AAA.kraugall for Sydney International Exhibition (Sydney, Australia: 1879)

redpajama_set_name: RedPajamaCommonCrawl


Well you won't believe this but I found the problem. This keyboard has ALT keys on both sides of the space bar. The one on the left works fine. Switches terminals and even takes me back to X. The ALT key on the right does nothing. How's that for strange!
Well I feel kinda stupid about the whole thing now but you're quite welcome. With my physical disabilities it's just easier to use the right one. And Right-CTRL-ALT-Fx does take you to the virtual terminal from X. It just doesn't do anything once you're in text mode.


Saginaw, Michigan - The Saginaw Spirit wrapped up the month of September with an exciting five-goal rally this past weekend that ended in an overtime finish at the Dow Event Center. While the Guelph Storm scored the final goal in overtime, it's a positive building block heading into a three-game road stand.
Looking to end a three-game winless streak that began on Sept. 22, scoring 12 total goals during that stretch, the Spirit will start a best of eight series in the Coors Light I-75 Divide Rivalry Series tonight against the Flint Firebirds. Puck drop is set for 7:00 p.m. (ET) at the Dort Federal Event Center. The Firebirds are experiencing their own respected early setback, allowing 26 goals through four consecutive losses, including a home opening 4-2 defeat to the London Knights last Saturday, their closest scoring difference so far this season.
The lone winless club across the OHL entering Wednesday, Flint allowed 12 goals to the Erie Otters after losing the season opener, 6-2, against the Kitchener Rangers. Before their clash with Saginaw, the Flint have responded to the letdowns by acquiring Lucas Rowe and Vladislav Kolyachonok.
Both roster additions were announced on Tuesday, with Rowe being traded from the Knights in exchange for a 2020 conditional third-round OHL draft pick. The former 18th overall selection in last year's draft played in 26 games for London, recording one goal and one assist.
Kolyachonok, having being claimed off waivers, played in one game for London this season after being taken in the second round of the 2018 CHL Import Draft, earning a point on Sept. 21 in a 5-2 win over the Windsor Spitfires.
Flint captain Ty Dellandrea, recently agreeing to a three-year, entry-level deal with the Dallas Stars as the 13th overall pick in the 2018 NHL Draft, obtained his first point of the season in the loss to London. The leading scorer for the Firebirds in 2017, Dellandrea finished with 59 points in the 20-win campaign.
The Firebirds went to two different goalies last month in Emanuel Vella and Luke Cavallin. Vella has stopped 74-of-90 shots with a save percentage of .822, recording the loss in three games. In three appearances for Cavallin, the 17-year-old has allowed an average of over five goals.
Saginaw and Flint will roll out a combined nine players having NHL ties with the Firebirds owning three in Dellandrea (Dallas), Dennis Busby (Arizona) and Fedor Gordeev (Toronto). The Spirit maintained its dominance over their in-state rival last season, winning seven games and losing once in extra time.
Sitting in fourth place in the OHL West Division standings with three points, winning its home opener against the Sault Ste. Marie Greyhounds on Sept. 19, Saginaw has seen an offensive rise from Albert Michnac, Cole Coskey and Nicholas Porco, the top three points leaders this season.
Coskey would score twice in the overtime loss to Guelph, including late in the third period which shortened the Spirit's deficit to one before Detroit Red Wings pick Brady Gilmour locked in the game-tying goal with eight seconds remaining in regulation.
Michnac has recorded three goals and four assists while Porco has enjoyed a three-game goal streak, collecting two points in the 7-5 loss to the Spitfire in the road opener.
Goaltender Ivan Prosvetov earned his first start in net on Saturday after making his OHL debut on Sept. 22 in the loss to the Sarnia Sting, replacing Cameron Lamour who got the win against the Greyhounds after making 23 saves.
Rookie Tristan Lennox has been reassigned to Milton Icehawks Jr. A on Monday, making his one appearance this season at Windsor, finishing with 12 saves.
The Spirit will next play back-to-back games this upcoming weekend, heading to Kitchener on Friday, Oct. 5, before visiting the Otters the following day. Flint will make its way to the Dow for the first time this year on Saturday, Oct. 20.


From his blistering British Invasion beginnings through his amazingly varied solo career right up to today, Jeff Beck has made the Stratocaster an integral part of his signature sound.
But apart from that, this is a fine guitar – a two piece alder body, a big maple neck with rosewood fingerboard, original Fender Gold Lace Sensor pickups in HSS configuration, and it's finished in fabulous Surf Green.
This lovely Jeff Beck Strat is super clean for its age. Big, beefy neck with the classic HSS pickup configuration – a real rock & blues monster. It is in excellent condition with only light player wear – very clean overall with some minor nicks & dings along with mild surface scratches.
Super beefy maple neck with cream side-dots. Beautiful dark rosewood fingerboard with cream dot inlays. Frets are in great shape with no visible wear. Sperzel locking tuners with a brushed steel finish. 1 5/8″ nut width; 25 1/2″ scale length.
The neck is straight & truss rod works fine. Jeff Beck Artist Signature decal is on the headstock. The actual real signature on the rear is labelled "1 of 3"— we believe that Fender Australia got Mr Beck to sign three of these models back in the day, and this is one of them.
The Jeff Beck Signature model normally sports an LSR roller nut which has been professionally replaced with vintage style bone nut on this one. It now has that great original look, and stills stays properly in tune. The original LSR nut is included in the sale, and could easily be re-installed if desired.
Contoured, solid alder body finished in Surf Green. Two-point tremolo bridge with adjustable saddles & original trem arm. 3-ply white pickguard. HSS Gold Lace Sensors with master volume, dual tone controls, 5-way selector switch & coil split switch. All electronics are in perfect working condition.
This JB Strat offers outstanding versatility, with a large palette of tonal possibilities. The 5-way switch in tandem with the coil-tapped bridge humbucker allows combinations to suit your every sonic need. The beefy maple neck is a great player, with a comfy medium low action.
This one is a superb player, with a cool look and great tone. We believe this "first edition" model will become collectable, as Fender changed the specs in the later version. This one is an excellent addition to any collection. Plus it offers bragging rights with that original JB signature !
Comes in its original Fender tweed case in good condition.


text:
Q: My C# Regex pattern fails to match text between tags I have the following raw text:
<target xml:lang="ar">افصل الدائرة عن مخرج جهاز التنفس،\nواترك خراطيم المهايئ الزفيري متصلة.</target>

And i'm interested in the text between the <target xml:lang="ar"> and the end tag </target> I realise it's a bad idea to match HTML or XML tags with Regexm but these tags are constants, as in there will never be added attributes (they are generated by some tool and will always be same)
Now I realise there's a million way to skin a cat, and that I can do a substring match to get text between > and < but it's really frustrating me why the pattern I chose isn't working, even though the online regex testers do match the text such as http://regexstorm.net/tester.
Here's my code:
string pattern = @"<target xml:lang=""ar"">(.*?)</target>";
string line = @"<target xml:lang=""ar"">افصل الدائرة عن مخرج جهاز التنفس،\nواترك خراطيم المهايئ الزفيري متصلة.</target>"
foreach (Match match in Regex.Matches(line, pattern))
{
    // Split the Arabic text from the xml tags
    string arabicTransMatch = match.Groups[1].Value;
    string[] xmlTags = line.Split(new string[] { arabicTransMatch }, StringSplitOptions.None);
    ...
}

Thanks heaps for your help all
Cheers,
Simon

A: Due to the frowned upon usage of Regex with Tags, I will answer my own question by stating that I've shied away from using Regex, and simply used the Substring method;
int startIndex = line.IndexOf(">") + 1;
line = line.Substring(startIndex, line.IndexOf("<", startIndex));

As for fixing the Regex matching issue, the advice given by @nhahtdh in regards to the SingleLine option did the trick.
Thanks for your comments guys.

redpajama_set_name: RedPajamaStackExchange


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I'm honoured to have recently been welcomed to the editorial board at www.flusserstudies.net, the on-line journal that publishes new research on Flusser's life and work.
My interest in the work of Vilém Flusser (1920-1991) dates back to 2003, the year I read the collection entitled Writings, edited by Andreas Strõhl. Since then I've translated three of his books and published some short pieces that trace particular implications of his thinking (see "c.v., "publications").


Each state runs its program differently, for more detailed information please visit their website here.
What Conditions are Screened For in Idaho?
Looking for resources? Check out our Newborn Screening Education and Training Resource Center.
The Idaho Legislature has instructed the Department of Health and Welfare to require that all babies born in Idaho receive screening tests for conditions that can result in intellectual disability or other serious health problems if they are not detected and treated soon after birth. This procedure is called the "newborn screen," or the "newborn blood spot screen." By detecting these metabolic, endocrine and hemoglobin conditions as well as cystic fibrosis, life-saving treatment can begin immediately.
Until the early 1990s, routine screening of newborns for inherited metabolic disorders was limited to three to five disorders. Today, using technology known as tandem mass spectrometry, more than 40 disorders of body chemistry can be detected in a single analysis of a small blood sample collected on special paper during the first few days of life.
This test is so important because it provides important information about your baby's health that you or even your doctor might not otherwise know. Most infants with conditions screened by this program show no obvious signs of disease immediately after birth. In each of these disorders there is an "invisible" problem in one of the many chemicals produced naturally in the baby's body. The Newborn Screening Program uses special laboratory tests to identify the infant who may have one of the disorders so that the baby's doctor can be alerted to the need for special care for the infant. Hopefully, this can be done before the condition has had time to cause damage. Early diagnoses and medical treatment usually can prevent complications such as intellectual disability or even death from these serious conditions.
Samples for testing must be collected before discharge from the hospital or birthing facility. A tiny sample of blood is obtained by pricking the baby's heel. The sample is placed on a special absorbent paper and is sent to the laboratory. Testing is done at the Oregon Public Health Laboratory. For infants born "out of hospital," the person responsible for registering the birth of the child also is responsible for assuring that a proper specimen is collected and submitted no later than 48 hours after birth.
Parents or guardians of babies need to be aware that a second test will be given and a filter paper test kit for that purpose will be provided when leaving the hospital or birthing facility. The second sample should be taken when your baby is more than 10 but less than 14 days of age. It can be taken at your doctor's office or at some hospitals and certain laboratories and health departments. After collection, the sample should be allowed to air dry and then mailed immediately in the envelope provided.
Your doctor or clinic will be informed when the tests are completed. Parents are notified only if there is a problem. If the doctor asks you to bring in your baby for retesting, do it as soon as possible! If your child does have a disorder, prompt action is very important. If you do not have a telephone, be sure to give your doctor the phone number of a friend, relative, or neighbor who can contact you. Also, be sure to notify your doctor immediately if you move after your baby is born. If your child should need to be retested, your doctor needs to know where to reach you. Remember, time is of great importance.
When you take your baby to the doctor for a regular checkup, ask the doctor about your newborn's results. It is important to remember that these tests simply provide information only about some uncommon conditions. An infant free of these disorders may have other medical problems for which these methods do not test. It is very important for your baby to have regular checkups and good general medical care.
Although Idaho does not have legislation requiring hearing screening, approximately 95% of all babies born in Idaho, and 99.3% of all babies born in Idaho hospitals, receive newborn hearing screening. Most midwives in Idaho are now able to provide hearing screenings, and free hearing screenings are available in every region for infants not born in a hospital. You can contact the Idaho Early Hearing Detection and Intervention program coordinator for assistance in locating a center.
How is Newborn Screening Paid for in Idaho?
As of July 2011, the cost of the two-specimen and NICU screening kit to medical providers is $100 total; $51 for the initial screen and $49 for the repeat screen. Cost coverage of this item will be determined by your insurance carrier or funding source.
While it is highly discouraged, parents in Idaho have the right to refuse the screening tests for their newborn infant if the testing conflicts with your religious beliefs. Please discuss this decision with your healthcare provider. If you decide to decline the screening, you will be asked to sign an "Informed Dissent" document that releases your healthcare provider from liability for whatever happens to your child due to lack of newborn screening.
One of the most common questions a family will face when told their child has a condition identified through newborn screening is wondering how they will afford specialized care for their newborn throughout life. Idaho has various agencies and laws, which will help provide the best, most specialized care for families in need.
In some circumstances, your doctor or other health care provider may be able to give you all the information you need. Other circumstances require services of a more highly trained professional. Genetic services, including genetic counseling, are available to Idaho residents with genetic or inherited diseases and their families. These services help families and their health care providers make informed decisions about their health care. Once a diagnosis is made, the next step is for a family to understand what the diagnosis means on a practical level. The geneticist or genetic counselor will explain how this condition has affected other people with the same diagnosis. Then they will use this information to help predict what kinds of symptoms or problems you or a family member may face in the future. Recent medical advances have created effective treatments for many genetic diseases. Some conditions have excellent treatment. Others have treatment that is experimental or controversial. At the end of a genetic evaluation, you should have a clear understanding of the available treatments for the genetic condition affecting your family. An appointment for genetic services in Idaho can be obtained at the St. Luke's Regional medical Center Genetics/Metabolic Clinic.
In addition to support from various state health agencies, Idaho residents covered by Medicaid will have their child's medical foods provided to them free of charge as long as they are medically necessary due to the condition preventing the use of traditional foods alone. The Children's Special Health Program Through the Title V Federal Grant provides some access to other foods and specialty care.
Your child's residual dried blood spot, which is what remains after the newborn screening tests are complete, may be stored at the laboratory for up to eighteen months. Without your written permission, the newborn screening specimen collected from your baby will never be used for anything other than retesting, diagnosis or quality assurance.
To see a copy of the blood spot card used in Idaho click here.


Source criticism (or information evaluation) is the process of evaluating an information source, i.e. a document, a person, a speech, a fingerprint, a photo, an observation or anything used in order to obtain knowledge. In relation to a given purpose, a given information source may be more or less valid, reliable or relevant. Broadly, "source criticism" is the interdisciplinary study of how information sources are evaluated for given tasks (cf. next sections).
1 The meaning of "source criticism"
The meaning of "source criticism"
Problems in translation: The Danish word "kildekritik" like the Norwegian word "kildekritikk" and the Swedish word "källkritik" derived from the German "Quellenkritik" and is closely associated with the German historian Leopold von Ranke (1795–1886). Hardtwig writes: "His [Ranke's] first work Geschichte der romanischen und germanischen Völker von 1494–1514 (History of the Latin and Teutonic Nations from 1494 to 1514) (1824) was a great success. It already showed some of the basic characteristics of his conception of Europe, and was of historiographical importance particularly because Ranke made an exemplary critical analysis of his sources in a separate volume, Zur Kritik neuerer Geschichtsschreiber (On the Critical Methods of Recent Historians). In this work he raised the method of textual criticism used in the late eighteenth century, particularly in classical philology to the standard method of scientific historical writing" (Hardtwig, 2001, p. 12739).
The larger part of the nineteenth and twentieth centuries would be dominated by the research-oriented conception of historical method of the so-called Historical School in Germany, led by historians as Leopold Ranke and Berthold Niebuhr. Their conception of history, long been regarded as the beginning of modern, `scientific' history, harked back to the `narrow' conception of historical method, limiting the methodical character of history to source criticism" (Lorenz, 2001).
Bible studies dominate the use of "source criticism" in America (cf. Hjørland, 2008). The term is thus relatively seldom used in English about historical methods and historiography (cf. Hjørland, 2008). This difference between European and American use of "source criticism" is somewhat strange considering the influence of Ranke on both sides of the Atlantic Ocean. It has been suggested that differences in the use of the term are not accidental but due to different views of the historical method. In the German/Scandinavian tradition this subject is seen as important, whereas the Anglo-American tradition it is believed that historical methods must be specific and associated with the subject studied, for which reason there is no general field of "source criticism".
In the Scandinavian countries and elsewhere source evaluation (or information evaluation) is also studied interdisciplinarily from many different points of view, partly caused by the influence of the Internet. It is a growing field in, among other fields, library and information science. In this context source criticism is studied from a broader perspective than just, for example, history or Biblical studies.
One distinction may be made between normative terms (such as source criticism) which prescribe methodological principles about the use of information sources and on the other hand descriptive terms like credibility, which tend to describe users' attitudes towards sources. These two aspects are, however, not always clearly separated.
"Media credibility and cognitive authority denote closely related concepts that are difficult to define unambiguously. This is partly because they overlap with a number of closely related concepts like quality of information, believability of media, and reliability and trustworthiness of information " (Savolainen, 2007).
"Information scientists tend to favour the concept of cognitive authority, while communication researchers prefer concepts such as source-, message-, medium- and media credibility". (Savolainen, 2007).
"Overall, cognitive authority was characterized as having six facets; trustworthiness, reliability, scholarliness, credibility, 'officialness' and authoritativeness; of these, trustworthiness was perceived as the primary facet. " (Savolainen, 2007).
"In turn, it is characteristic of studies on media credibility that they focus on the channel through which the content is delivered [...]. Typically, these studies have explored the criteria by which diverse media such as newspapers, radio and television are perceived as believable sources of information. As early as in the 1950s, regular surveys of media credibility were conducted in the United States by asking respondents to indicate which medium they would believe if they got conflicting reports of the same news story from radio, television, magazines and newspapers". (Savolainen, 2007).
"An empirical survey conducted in the late 1990s in Germany revealed that the credibility of the Web was fairly high among the general public, although printed newspapers were rated ahead of it [reference omitted here]. Compared to the Web, newspapers were perceived as more clear, serious, thorough, detailed, critical, generally credible, balanced, competent and professional. With regard to these qualities, the differences between television and the Web were less significant. The Web was conceived of as more up-to-date than newspaper and television. On the one hand, newspapers were considered more biased than television and the Web. This is due to the fact that although most newspapers call themselves neutral they nevertheless do have a political bias. On the other hand, the greater bias of newspapers may be seen as positive since they articulate alternative positions in public discourse. Interestingly, when asked which medium they would prefer in the case of contradictory news on the same issue, the respondents would mainly place their trust in traditional media." (Savolainen, 2007).
Human sources may be relics (e.g. a fingerprint) or narratives (e.g. a statement or a letter). Relics are more credible sources than narratives.
A primary source is more reliable than a secondary source, which in turn is more reliable than a tertiary source and so on.
"Because each source teaches you more and more about your subject, you will be able to judge with ever-increasing precision the usefulness and value of any prospective source. In other words, the more you know about the subject, the more precisely you can identify what you must still find out". (Bazerman, 1995, p. 304).
The reliability of a given source is relative to the questions put to it.
"The empirical case study showed that most people find it difficult to assess questions of cognitive authority and media credibility in a general sense, for example, by comparing the overall credibility of newspapers and the Internet. Thus these assessments tend to be situationally sensitive. Newspapers, television and the Internet were frequently used as sources of orienting information, but their credibility varied depending on the actual topic at hand" (Savolainen, 2007).
How was the source located?
Who is the author and what are the qualifications of the author in regard to the topic that is discussed?
In which country was it published?
Does the source show a particular cultural or political bias?
Does the source contain a bibliography?
Has the material been reviewed by a group of peers, or has it been edited?
How does the article/book compare with similar articles/books?
How general are principles of source criticism? Some principles are universal, other principles are specific for certain kinds of information sources. One may ask whether principles of source criticism are unique to the humanities?
There is today no consensus about the similarities and differences between natural science and humanities. Logical positivism claimed that all fields of knowledge were based on the same principles. Much of the criticism of logical positivism claimed that positivism is the basis of the sciences, whereas hermeneutics is the basis of the humanities. This was, for example, the position of Jürgen Habermas. A newer position, in accordance with, among others, Hans-Georg Gadamer and Thomas Kuhn understands both science and humanities as determined by researchers' preunderstanding and paradigms. Hermeneutics is thus a universal theory. The difference is, however, that the sources of the humanities are themselves products of human interests and preunderstanding, whereas the sources of the natural sciences are not. Humanities are thus "doubly hermeneutic".
Natural scientists, however, are also using human products (such as scientific papers) which are products of preunderstanding (and, for example, academic fraud).
Epistemological theories are the basic theories about how knowledge is obtained and thus the most general theories about how to evaluate information sources. Empiricism evaluates sources by considering the observations (or sensations) on which they are based. Sources without basis in experience are not seen as valid. Rationalism provides low priority to sources based on observations. In order to be meaningful observations must be grasped by clear ideas or concepts. It is the logical structure and the well definedness that is in focus in evaluating information sources from the rationalist point of view. Historicism evaluates information sources on the basis of their reflection of their sociocultural context and their theoretical development. Pragmatism evaluate sources on the basis of how their values and usefulness to accomplish certain outcomes. Pragmatism is skeptical about claimed neutral information sources.
The evaluation of knowledge or information sources cannot be more certain than is the construction of knowledge. If we accept the principle of fallibilism we also have to accept that source criticism can never 100% verify knowledge claims. As discussed in the next section is source criticism intimately linked to scientific methods.
The presence of fallacies of argument in sources is another kind of philosophical criteria for evaluating sources. Fallacies are presented by Walton (1998). Among the fallacies are the 'ad hominem fallacy' (the use of personal attack to try to undermine or refute a person's argument) and the 'straw man fallacy' (when one arguer misrepresents another's position to make it appear less plausible than it really is, in order more easily to criticize or refute it.) See also fallacy.
Research methods are methods used to produce scholarly knowledge. The methods that are relevant for producing knowledge are also relevant for evaluating knowledge. An example of a book that turns methodology upside-down and uses it to evaluate produced knowledge is Katzer; Cook & Crouch (1998). See also Unobtrusive measures, Triangulation (social science).
Studies of quality evaluation processes such as peer review, book reviews and of the normative criteria used in evaluation of scientific and scholarly research. Another field is the study of Scientific misconduct.
Harris (1979) provides a case study of how a famous experiment in psychology, Little Albert, has been distorted throughout the history of psychology, starting with the author (Watson) himself, general textbook authors, behavior therapists, and a prominent learning theorist. Harris proposes possible causes for these distortions and analyzes the Albert study as an example of myth making in the history of psychology. Studies of this kind may be regarded a special kind of reception history (how Watson's paper was received). It may also be regarded as a kind of critical history (opposed to ceremonial history of psychology, cf. Harris, 1980). Such studies are important for source criticism in revealing the bias introduced by referring to classical studies.
See also Hjørland (2008): Empirical studies of the quality of science.
Textual criticism (or broader: text philology) is a part of philology, which is not just devoted to the study of texts, but also to edit and produce "scientific editions", "scholarly editions", "standard editions", "historical editions", "reliable editions", "reliable texts", "text editions" or "critical editions", which are editions in which careful scholarship has been employed to ensure that the information contained within is as close to the author's/composer's original intentions as possible (and which allows the user to compare and judge changes in editions published under influence by the author/composer). The relation between these kinds of works and the concept "source criticism" is evident in Danish, where they may be termed "kildekritisk udgave" (directly translated "source critical edition").
In other words it is assumed that most editions of a given works is filled with noise and errors provided by publishers, why it is important to produce "scholarly editions". The work provided by text philology is an important part of source criticism in the humanities.
The study of eyewitness testimony is an important field of study used, among other purposes, to evaluate testimony in courts. The basics of eyewitness fallibility includes factors such as poor viewing conditions, brief exposure, and stress. More subtle factors, such as expectations, biases, and personal stereotypes can intervene to create erroneous reports. Loftus (1996) discuss all such factors and also shows that eyewitness memory is chronically inaccurate in surprising ways. An ingenious series of experiments reveals that memory can be radically altered by the way an eyewitness is questioned after the fact. New memories can be implanted and old ones unconsciously altered under interrogation.
Anderson (1978) and Anderson & Pichert (1977) reported an elegant experiment demonstrating how change in perspective affected people's ability to recall information that was unrecallable from another perspective.
In psychoanalysis the concept of defence mechanism is important and may be considered a contribution to the theory of source criticism because it explains psychological mechanisms, which distort the reliability of human information sources.
In schools of library and information science (LIS) is source criticism of taught as part of the growing field Information literacy. Study issues like relevance, quality indicators for documents, kinds of documents and their qualities (e.g. scholarly editions) and related issues are studied in LIS and are relevant for source criticism. Bibliometrics is often used to find the most influential journal, authors, countries and institutions. The study of book reviews and their function in evaluating books should also be mentioned. The well-known comparison of Wikipedia and Encyclopædia Britannica (Giles, 2005) - although not done by information scientists - contained an interview with an information scientist (Michael Twidale) and should be obvious to include in LIS.
It could be argued that library and information education should provide teaching in source criticism at least at the same level as is taught in Upper Secondary School (see Gudmundsson, 2007).
In library and information science the checklist approach has often been used. A criticism of this approach is given by Meola (2004): "Chucking the checklist".
Libraries sometimes provide advices on how their users may evaluate sources.
The Library of Congress has a "Teaching with Primary Sources" (TPS) program.
Source criticism is also about ethical behavior and culture. It is about a free press and an open society, including the protecting information sources from being persecuted (cf., Whistleblower).
Photos are often manipulated during wars and for political purposes. One well known example is Joseph Stalin's manipulation of a photograph from May 5, 1920 on which Stalin's predecessor Lenin held a speech for Soviet troops that Leon Trotsky attended. Stalin had later Trotsky retouched out of this photograph. (cf. King, 1997). A recent example is reported by Healy (2008) about North Korean leader Kim Jong Il.
Much interest in evaluating Internet sources (such as Wikipedia) is reflected in the scholarly literature of Library and information science and in other fields. Mintz (2002) is an edited volume about this issue.
The term Internet epistemology is among newly suggested terms.
Examples of literature examining Internet sources include Chesney (2006), Fritch & Cromwell (2001), Leth & Thurén (2000) and Wilkinson, Bennett, & Oliver (1997).
Special topics such as the reliability of search engines and Wikipedia have their own investigations.
The scientific journal Nature compared Wikipedia with Encyclopædia Britannica. (See Giles, 2005) Encyclopædia Britannica replied (2006). The German magazine Stern compared Wikipedia with leading German Encyclopedias (Sterns test of Wikipedia).
"In history, the term historical method was first introduced in a systematic way in the sixteenth century by Jean Bodin in his treatise of source criticism, Methodus ad facilem historiarium cognitionem (1566). Characteristically, Bodin's treatise intended to establish the ways by which reliable knowledge of the past could be established by checking sources against one another and by so assessing the reliability of the information conveyed by them, relating them to the interests involved." (Lorenz, 2001, p. 6870).
As written above, modern source criticism in history is closely associated with the German historian Leopold von Ranke (1795–1886), who influenced historical methods on both sides of the Atlantic Ocean, although in rather different ways. American history developed in a more empirist and antiphilosophical way (cf., Novick, 1988).
Gudmundsson (2007, p. 38) writes: "Source criticism should not totally dominate later courses. Other important perspectives, for example, philosophy of history/view of history, should not suffer by being neglected" (Translated by BH). This quote makes a distinction between source criticism on the one hand and historical philosophy on the other hand. However, different views of history and different specific theories about the field being studied may have important consequences for how sources are selected, interpreted and used. Feminist scholars may, for example, select sources made by women and may interpret sources from a feminist perspective. Epistemology should thus be considered a part of source criticism. It is in particular related to "tendency analysis".
In archaeology, radiocarbon dating is an important technique to establish the age of information sources. Methods of this kind were the ideal when history established itself as both a scientific discipline and as a profession based on "scientific" principles in the last part of the 1880s (although radiocarbon dating is a more recent example of such methods). The empiricist movement in history brought along both "source criticism" as a research method and also in many countries large scale publishing efforts to make valid editions of "source materials" such as important letters and official documents (e.g. as facsimiles or transcriptions).
Historiography and Historical method include the study of the reliability of the sources used, in terms of, for example, authorship, credibility of the author, and the authenticity or corruption of the text.
Brundage (2007) and Howell & Prevenier (2001) provide introductions to the field.
The responsibility of the connoisseur is, besides appraising quality, attributing authorship, supplying a date and verifying authenticity of works of art. Many research methods are used. For example, detailed knowledge about the colors, papers, and other materials used by artists is systematically collected by the connoisseur. Not only from what factory a piece of paper was made and when it was made, but also where the artist bought it and how often and how much he used to buy. By combining many kinds of evidence in this way an empirical argument about the age of a given work may be established.
Although the term "source criticism" is not used in this domain has the reliability of observers been carefully studied in association with the concept personal equation.
Source criticism, as the term is used in biblical criticism, refers to the attempt to establish the sources used by the author and/or redactor of the final text. The term "literary criticism" is occasionally used as a synonym.
Biblical source criticism originated in the 18th century with the work of Jean Astruc, who adapted the methods already developed for investigating the texts of Classical antiquity (Homer's Iliad in particular) to his own investigation into the sources of the Book of Genesis. It was subsequently considerably developed by German scholars in what was known as "the Higher Criticism", a term no longer in widespread use. The ultimate aim of these scholars was to reconstruct the history of the biblical text, as well as the religious history of ancient Israel.
Related to Source Criticism is Redaction Criticism which seeks to determine how and why the redactor (editor) put the sources together the way he did. Also related is form criticism and tradition history which try to reconstruct the oral prehistory behind the identified written sources.
Journalists often work with strong time pressure and have access to only a limited number of information sources such as news bureaus, persons which may be interviewed, newspapers, journals and so on (see journalism sourcing). Journalists' possibility for conducting serious source criticism is thus limited compared to, for example, historians' possibilities.
The most important legal sources are created by parliaments, governments, courts, and legal researchers. They may be written or unformal and based on established practices.
In assessing the relative value of different kinds of information sources and evidence are court decisions always decisive — directly or indirectly. The discussion of the relevance and importance of kinds of sources must be seen as what kind of evidence is most important in court rooms, both in a descriptive way (what do courtrooms actually use) and in a normative way (what should courtrooms ideally use). Although legal information is mostly used outside courtrooms, its relevance and validity is tested by its use in courtrooms or as thought esperiments: What would be the case if tried in court.
Different views concerning the quality of different sources is related to different legal philosophies: Legal positivism is the view that the text of the law should be considered in isolation, while legal realism, interpretivism (legal), critical legal studies and feminist legal criticism interprets the law on a broader cultural basis.
In medicine there is today a strong school of thought termed "evidence based medicine" (EBM). Here, some very explicit criteria have been developed on how to evaluate documents, including a hierarchy of evidence. EBM may thus be seen as a theory about source evaluation in medicine (a theory connected with empiricism).
Riegelman (2004) Studying a Study and Testing a Test: How to Read the Medical Evidence. Is a general text about critical reading in medicine.
^ Hjørland, Birger (2012). Methods for evaluating information sources: An annotated catalogue. Journal of information science. 38(3), 258-268.
^ Balin, A. & Grafstein, A. (2010). The critical assessment of research: Traditional and new methods of evaluation. Oxford: Chandos Publishing.
^ Healy, Jack (2008-11-07). "Was the Dear Leader Photoshopped In?". The New York Times.
^ Verhoeven, Gerrit (2012). Mastering the connoisseur's eye: Paintings, Criticism, and the Canon in Dutch and Flemish travel culture (1600-1750). Eighteenth-Century Studies, 46(1), 29-56.
Gudmundsson, David (2007). När kritiska elever är målet. Att undervisa i källkritik på gymnasiet. [When the Goal is Critical Students. Teaching Source Criticism in Upper Secondary School]. Malmö, Sweden: Malmö högskola. Full text Invalid language code.
Hjørland, Birger (2008). Source criticism. In: Epistemological Lifeboat. Ed. by Birger Hjørland & Jeppe Nicolaisen.
Leth, Göran & Thurén, Torsten (2000). Källkritik för internet . Stockholm: Styrelsen för Psykologiskt Försvar. (Hentet 2007-11-30).
"Wikipedia: Testsieg und Verschwörungen" [Sterns test of Wikipedia]. Heise Online (in German). 5 December 2007.
40x40px Look up quellenforschung in Wiktionary, the free dictionary.


text:
Sudan's President Bashir 'siphoned off millions' - ICC
Image caption Sudan has denied allegations that Mr Bashir stole public funds
Sudanese President Omar al-Bashir has been accused of siphoning off up to $9bn (£5.6bn; 7bn euros) of his country's funds by the chief prosecutor of the International Criminal Court (ICC).
Luis Moreno Ocampo told the BBC that President Bashir had hidden the money in personal accounts outside Sudan.
Mr Ocampo's suspicions originally came to light when a diplomatic cable obtained by Wikileaks was published by the Guardian newspaper.
Sudan has forcefully denied the claims.
The ICC's chief prosecutor has charged Mr Bashir with crimes against humanity, war crimes and genocide over alleged atrocities in Sudan's Darfur region.
'Not in London'
Mr Ocampo told the BBC he had looked into Mr Bashir's financial affairs as part of the overall case against him.
He said the court had "strong reason to believe that Bashir has a lot of money" held in personal accounts outside Sudan - but that he could not be sure of the precise amount, with estimates ranging from hundreds of millions of dollars up to $9bn.
Ocampo suggested if Bashir's stash of money were disclosed (he put the figure at possibly $9 billion), it would change Sudanese public opinion from him being a 'crusader' to that of a thief
Senior US diplomat, author of cable revealed by Wikileaks
In the leaked diplomatic cable, US diplomats report Mr Ocampo as saying that "Lloyd's Bank in London might be holding or knowledgeable of the whereabouts of his money".
But Lloyd's has denied holding any funds in Mr Bashir's name, and in his BBC interview, Mr Ocampo agreed that the money was not held in a London account. "This is a confusion," he said, and he said he did not know where the money was.
"The money is not in UK and it's sad because in UK it would be easy to get the money. In UK, some banks [have] official accounts of the Sudanese government - that's different. The personal accounts of President Bashir are not there."
Asked why he did not reveal his suspicions about siphoned funds at the time the ICC issued an arrest warrant for Mr Bashir in March 2009, Mr Ocampo said he was not bringing financial charges against Mr Bashir but that any funds uncovered could be used to compensate his victims.
Correspondents say that if Mr Bashir does indeed hold a fortune of $9bn in secret bank accounts, that would be equivalent to one tenth of the country's annual GDP.
"Ocampo suggested if Bashir's stash of money were disclosed... it would change Sudanese public opinion from him being a 'crusader' to that of a thief," one senior US official was quoted as saying in the leaked cable.
'No credibility'
Speaking to the BBC, a spokesperson for the Sudanese government, Dr Khalid al-Mubarak, dismissed the claims made by Mr Ocampo.
"I know that we have a government, we have a treasury, we have a system, we have a civil service," Dr Mubarak said.
"And that we are not the sort of country in which the president puts all the money under his pillow and decides to deal with it the way he does... We are a country with rules and regulations, and a civil service."
He said Mr Ocampo had "lost all credibility as far as Sudan is concerned. He has been proven wrong more than once about Sudan and he has exaggerated many things about Sudan.
"And this is the reason why Sudan as a whole is being targeted," Mr Mubarak said.
At a glance: Wikileaks cables
ICC indictment of Sudanese leader
Darfur warrant for Sudan's Bashir: ICC adds genocide
Deadly Darfur
Government of Sudan


Canada's economy may have hit the skids in June but house prices across the country still jumped almost 2%, the biggest one-month increase in two years, the latest Teranet-National Bank National Composite House Price Index report said yesterday.
Canadian house prices were up 1.7% in June compared with the previous month, the biggest month-on-month jump since August 2009 taking the index to a new all-time high of 144.27, the report said.
This is the third straight monthly increase of more than 1% and the seventh straight rise in a row. The index is also up 4.5% compared with a year ago.
The news comes the same day Statistics Canada reported the Canadian economy actually shrank 0.4% annualized in the second quarter, the first contraction since mid-2009.
Prices were up in all six major metropolitan markets surveyed, with Toronto leading the pack at a 2.0% increase. Vancouver and Ottawa came in at +1.7%, while Calgary posted a 1.6% rise, Montreal +1.1% and Halifax +1.0%.
This is the ninth-straight monthly increase for Vancouver, and all-time index highs for five of the six cities.
Calgary is 10.9% off its all-time high in August 2007.
Since Teranet first started tracking prices in June 2005 with a base level of 100, home prices have jumped 44.27%.
The Vancouver index leads the pack at 167.77, suggesting prices have gone up 67.77% since 2005.
Toronto, meanwhile, has the lowest index rating at 131.26, meaning prices have accelerated only 31.26% in that time.


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