RETRO KIMMER'S BLOG: GREASE BEHIND CLOSED DOORS TOMORROW ON REELZ!
GREASE BEHIND CLOSED DOORS TOMORROW ON REELZ!
Grease is the word. Without question the hit movie is an American touchstone loved by audiences young and old for the last 40 years. But before its 1978 release no one foresaw that a $6 million movie dismissed as "cinematic cotton candy" would become the highest-grossing movie musical of the 20th century and produce the top-selling movie soundtrack in history.
LOOKING FORWARD TO PRINCESS EUGENIE'S WEDDING!
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THE CROWN: IMAGINING A ROYAL WORLD EXHIBIT!


Inorganic chemistry is a division of chemistry that studies the sources, preparations, structures, natures, changes and applications of research elements, simple substances and inorganic compounds. The researches and solutions of the basic scientific questions of inorganic chemistry in the fields of materials, life, energies, information and environment are the important research contents.
The subject of inorganic chemistry received the right to grant master's degree in 2003, and received the right to grant doctor's degree in 2005. In 2007 this subject was declared Municipal Key Discipline in Beijing successfully. The department of inorganic chemistry of our College of Science in our university undertakes the construction assignment of the discipline of inorganic chemistry. At present there are 15 teaching and administrative staff, among whom there are 3 full professors, 8 vice professors, 4 doctoral supervisors, 14 people who have doctorates and 2 people who have been awarded the title of "New Century Excellent Talents".
The department of inorganic chemistry is in charge of the basic course teaching of inorganic chemistry of the College of Science. It also bears the teaching jobs of the basic courses including Basic Chemistry, College Chemistry and Analytical Chemistry, the basic professional curriculum including Inorganic Synthesis and the Development of Modern Instrument Analysis and the graduate courses including Advanced Inorganic Chemistry, Applied Electrochemistry, and Chemical and Biological Sensing Technology. At the mean time, our department also undertakes the tasks to guide graduate design for undergraduates and to guide the graduate students to carry out scientific researches. The teachers of our department devote themselves completely to the education and educational reforms. They also participate in many national-and-school-level teaching reform projects. Many of the teachers have won the teaching achievement prizes of Beijing and school level. The subject of Inorganic Chemistry is rated as the top-quality course of school level, school-level bi-lingual model course and national bi-lingual model course of Ministry of Education in 2010.
After many years' development, the Department of Inorganic Chemistry of BUCT has formed four characteristic research directions including "Intercalation Chemistry", "Chemistry of micro-Nano Materials", "Chemistry of Functional Materials Assembly" and "Coordination Chemistry". The teachers of our apartment bear many projects of National Natural Science Foundation of China, provincial scientific research projects and crossing research projects. In the fields of energy conversion and energy storage materials, electrochemical transducer and testing technology, the synthesis, separation and assembly of functional colloidal nanoparticles, inorganic nano functional materials and the researches of catalyst and absorbing materials, they yield substantial results. On the internationally famous journals including Angew. Chem. Int. Edit., J. Am. Chem. Soc., ACS Nano., Chem. Commun. and Biosensor Bioelectron, the teachers have published a large number of scientific papers. They also have applied many international and national invention patents. Some of the patents have got practical applications in chemical industry production, achieving certain economic and social benefits.


Frances MaddenLast public show for 2017!
Last public show for 2017!
We had a blast performing this past weekend at the annual Wangaratta Jazz Festival, which marked the end of our East Coast Tour including Sydney, Melbourne, Hobart and Brisbane. Thank you to all who came along to our shows, it's been so much fun to perform for you and we promise to visit again soon!
Tickets available HERE, bookings highly recommended.
PS. Can't make it on the 18th but would like to see a show? We'll be back at The Basement on Feb 24th 2018. Save the date!


text:
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text:
\section{Introduction} \label{introd}

GX~339--4 (also called V821 Ara) is a recurrent black hole transient X-ray binary
(i.e. this source undergoes frequent outbursts followed by very faint states) with few episodes
in quiescence (e.g. \cite{kong00}). \citet{hynes03} determined, on the basis of optical spectroscopic
observations, that this source has an orbital period of 1.7 days and a mass
function of $f(M)=5.8{\pm}0.5\,M_{\odot}$ (since $f(M){\propto}M\sin^3(i)$, note that this represents
a lower limit to the black hole mass). The
distance and the spectral type of the secondary star are uncertain. \citet{hynes04} established the distance to be
6-15\,kpc depending on the spectral type of the secondary (a subgiant), being later than F spectral type.
Therefore, this black hole transient is a low-mass X-ray binary (LMXB). Slightly later,
on the basis of binary parameters determination,
\citet{zdziarski04} suggested the distance to be ${\gtrsim}7$\,kpc, consistent with \citet{hynes04}.
The inclination of this binary system is known to be low,
from the small emission-line velocity amplitudes observed. \citet{wu01} determined a plausible value for the
inclination of $i=15^{\circ}$ from spectroscopic data.
\citet{miller04a}, \citet{miller04b} and \citet{miller06a} found that fits of the relativistic Fe $K_{\alpha}$ line
imply a very low value of the inclination ($i=20-30^{\circ}$) as well. The latter corresponds to
the inner disk inclination, i.e. not the inclination of the binary plane.

The timing and spectral properties of GX~339--4 required a
re-interpretation of the standard classification scheme of the black hole states. The behavior of
GX~339--4 supports the view that, as reviewed by \citet{homan01} and \citet{klis06}, X-ray states are important, but are
not a simple function of the luminosity. As claimed by \citet{homan05}, another variable apart from the mass accretion
rate, $\dot{M}$, drives black hole state transitions
and at least two factors must drive state transitions; the second factor may be, e.g., the compactness of the
corona (\citet{homan01}). Black hole X-ray transients and related states (\citet{tanaka95}; \citet{chen97}; \citet{mcclintock06})
provide an excellent opportunity to investigate the importance of irradiation and non-thermal processes in the
X-${\gamma}$-ray spectra of X-ray binaries.
Black hole binary outbursts typically begin and end in the low/hard
state, with a high-energy spectrum that can be roughly described by a powerlaw with a spectral index
${\Gamma}$ varying in the range 1.4-2.1. At some point in the outburst (coinciding with
the presence of radio outflows) the source transits from the hard intermediate (HIMS) to soft intermediate (SIMS) states, characterized
by a quenching of the radio emission (i.e. the so-called jet line). Then, the thermal disk component luminosity increases
and the high energy powerlaw is softer (${\Gamma}=1.5-2.5$) (\citet{miyamoto91a}, \citet{belloni97}, \citet{homanbell05}, see \citet{klis06}
for a review). The transition between these states occurs very rapidly; they were
found in {\it EXOSAT} observations of GX~339--4 by \citet{mendez97}. The Very/High
(hereafter VH) state was first observed in GX~339--4 \citep{miyamoto91a}, when very peculiar X-ray
variability was detected with {\it Ginga/LAC} (6\,Hz QPO, 10-60\,s duration dips and "flip-flops").
\citet{miyamoto91b} even
proposed a jet model in order to account for the observed time variability in this state, on the basis of
the size of the Comptonizing coronae inferred from observations of GX~339--4 in the VH state \citep{miyamoto91a}.
Recent studies (\citet{homan01}, \citet{mendez97}, \citet{wolt07}) point out that the VH state is
really an intermediate state but at a different luminosity level.

Since its diskovery more than 30 years ago by \citet{markert73}, the source has been extensively studied with several
optical, infrared, X-ray and ${\gamma}$-ray observatories. At higher energy its emission has been studied
by all the major observatories, i.e., {\it GRANAT/SIGMA} (\citet{grebenev93}, \citet{bouchet93}), {\it CGRO/OSSE} \citep{grabelsky95},
{\it CGRO/BATSE} (\citet{harmon94}, \citet{rubin98}), {\it ASCA} (\citet{wilms99}),
{\it Ginga} (\citet{ebisawa93} and \citet{ueda94}), {\it RXTE} (e.g. \citet{zdziarski04}, \citet{belloni99}) and {\it INTEGRAL} (\citet{joinet06},
\citet{belloni06}). \citet{homan05} presented a multi-wavelength
study of the 2002 outburst and suggested a non-thermal jet origin for the optical/near-infrared emission
in the low/hard state, while the accretion disk dominates in the high/soft state. This source is very intriguing
in the optical, since its photometric optical behavior shows a very low amplitude modulation superposed
by some flickering events. In addition to the QPOs detected in X-rays (usually appearing in the low/hard state
and maintained in the intermediate states, while quenched in the high/soft state; see e.g. \citet{belloni05}),
this source also shows optical QPOs (${\rm f}{\approx}0.064$\,Hz; \citet{motch82}, \citet{steiman-cameron97}). A very
interesting issue is also the occurrence of optical states corresponding to the X-ray states (\citet{motch83}, \citet{motch85}).
This kind of variability is difficult to explain if optical radiation comes from reprocessing of X-rays and
seems to demands optical activity originated in the base of a jet.

GX~339--4 may harbor a black hole with a high spin parameter. \citet{miller04a} and \citet{reis08} found
very small inner disk radius of $2-3\,{\rm R_g}$
(where $R_{g}=GM/c^{2}$ and $a=cJ/GM^{2}$; see \citet{bardeen72} and \citet{thorne74}), implying
a dimensionless spin parameter of $a>0.8-0.9$ \citep{miller06a}. Relativistic radio jets with $v/c>0.9$
have recently been observed, detected \citep{gallo04} during a transition from the low/hard to the high/soft
state, therefore increasing the list
of known microquasars showing similar radio and X-ray properties. A radio jet is usually reported in the
low/hard state of GX~339--4, for which \citet{fender99} reported a quenching
of the radio emission during the high/soft state (by a factor of ${\geq}25$ compared to the low/hard state).
The low/hard state would be associated by a steady state of the outflow (\citet{corbel00}, \citet{fender01}, \citet{gallo03}).
It was also proposed that during state transitions the radio emission results in one or more discrete ejection
events, as already observed by \citet{gallo04} during their detection of jets. GX~339--4 shares X-ray
timing and spectral properties with the classical black hole Cyg~X-1, although the former exhibits more
frequent state changes and a larger dynamic range of soft X-ray luminosity (\citet{tanaka95},\citet{zdziarski98},
\citet{nowak99}).

While the physical nature of the soft component is commonly
associated with an optically thick accretion disk, there is no consensus about the origin of the hard
powerlaw component, where a powerlaw is probably a simplification of a much more complex reality. The
energy spectra include also additional components, important for the physics of accretion, such as
the Fe $K_{\alpha}$ fluorescence feature (see, e.g., \citet{miller07}, \citet{reynolds03}) and
Compton reflection bump, both being different aspects of the same physical
origin (i.e. fluorescence of the Fe ions and Compton back-scattering, respectively, both being the most obvious
reactions of an irradiated disk by a high-energy source; \citet{george91}).
An extremely high ionisation may inhibit the formation of emission and
absorption lines in the inner disk, which would explain the lack of Fe $K_{\alpha}$ fluorescence
emission line in some systems. One important
parameter to measure is the presence/absence of a high energy cut-off in the spectrum, for which
observations at energies $>20$\,keV are necessary. It is known since a long time (\citet{sunyaev80},\citet{grove98}) that
the spectrum in the low/hard state show a cut-off around $100$\,keV. This cut-off was interpreted
as being a consequence of the thermal (inverse) Comptonization of photons from the disk on a distribution of electrons
thought to represent a corona (for which the geometry is a matter of debate).

In this paper we report on spectral analysis of simultaneous {\it INTEGRAL} and XMM/EPIC-pn data, during five and
three Target of Opportunity observations of GX~339--4, respectively, occurring between 2007 January 30 and March 31
(epochs 1--5 below; see Table \ref{tobserv} for more details). We fit the obtained spectra with phenomenological models in Section \ref{spec_phenom} and
we observed that the source spectral states evolved from one observation to the other, as reported in Section \ref{state_class}.
Fits of the spectrum with both phenomenological and Comptonization models are presented in
Section \ref{spec_phenom}, \ref{spec_eqpair} and \ref{spec_excess} and we end with the discussion of the results in Section \ref{discuss}.

\section{Observations} \label{observ}

In 2006 November, X-ray activity of GX~339--4 was detected with the Rossi X-ray Timing Explorer (RXTE;
\citet{swank06:atel944}). The source had an almost constant flux until end of December 2006,
when the hard (15-50\,keV) X-ray flux increased by a large amount. It reached its brightest level
since 2004 November, as detected by SWIFT/BAT \citep{krimm:atel968}.
At the end of January 2007, observations were triggered with the {\it INTEGRAL} satellite \citep{miller:atel980}.
During the following months, the source underwent an evolution from the low/hard to softer states, as shown in
preliminary results reported in Caballero-Garcia et~al. 2007a-e.
Observations in radio with ATCA during February 4 to 18 revealed that the source was undergoing a series of plasma
ejection events \citep{corbel07}. Our {\it INTEGRAL} observations cover 5 Target of Opportunity
observations of ${\approx}130$\,ks each, spread from 2007 January 30 to March 31 (see Table \ref{tobserv}).
We also carried out a series of 3 ToO observations with the {\it XMM-Newton} satellite, simultaneous with the second, third and
fifth {\it INTEGRAL} observations. Details about the dates and exposure times appear in Table \ref{tobserv}.

\subsection{INTEGRAL} \label{ins:integral}

The data described were obtained with {\it INTEGRAL},
using the following instruments: the SPectrometer on
{\it INTEGRAL} (SPI; \citet{vedrenne03}), the {\it INTEGRAL} IBIS Soft Gamma-Ray Imager
(ISGRI; \citet{lebrun03}) and the Joint European X-ray Monitor (JEM-X;
\citet{lund03}. SPI, ISGRI and JEM-X allow
images to be obtained through the coded mask technique.
ISGRI is optimized for 15\,keV to 1\,MeV imaging
and SPI is optimized for high-resolution spectroscopy in the 18\,keV
to 8 MeV band. The former provides an angular resolution of $12'$
full-width half maximum (FWHM) and an energy resolution, $E/{\Delta}E$
of ${\approx}12$ (FWHM) at 100\,keV. SPI provides an angular
resolution of $2.8^{\circ}$ (FWHM) and an $E/{\Delta}E$ of $430$ FWHM
at 1.3 MeV. JEM-X has a fully coded Field of View (FOV) of
$4.8^{\circ}$ diameter and an angular resolution of $3'$ FWHM, with a
spectral resolution of 1.2\,keV (FWHM) at 10\,keV. JEM-X
has a spectral resolution of $E/{\Delta}E=0.2$ at 6\,keV, thus providing medium
resolution spectral capabilities in the energy range of 3--35\,keV.

The difference
in the (effective) exposure times between the {\it INTEGRAL} instruments given in Table
\ref{tobserv} (JEM-X, ISGRI and SPI) are due to the difference in the
dead times and variation in the efficiency along the fields of view.
The dithering pattern used during the observations was $5{\times}5$
(square of 25 pointings separated by 2.17 degrees centered on the main
target of the observation); this is the best pattern in order to
minimize background effects for the SPI and ISGRI instruments in
crowded fields. Data reduction was performed using the standard Off-line Science Analysis (OSA) 7.0
software package available from the {\it INTEGRAL} Science Data Centre
(ISDC).

Because of the steep fall in response off-axis in the case of JEM-X, and because of its
reduced FOV (${\approx}5^{\circ}$ of diameter), we limited the
pointing radius with respect to the GX~339--4 position to be
within $4^{\circ}$. In the case of SPI and ISGRI, with large Fully
Coded Fields of Views (FCFOV) ($16^{\circ}{\times}16^{\circ}$ for SPI
and $9^{\circ}{\times}9^{\circ}$ for ISGRI), pointing selections
were not necessary. In total, 149, 254 and 107 pointings (or Science
Window -- each having exposure times lasting from 1800 to 3600 s)
data were used for SPI, ISGRI and JEM-X, respectively.
The difference in the number of pointings between SPI and ISGRI is due
to the fact that in epoch 4 and 5 the source was too weak in hard X-rays
($E>20$\,keV) to be detected with SPI. Due to the fact that SPI is a high resolution
spectrograph in its energy range (20-8\,000\,keV), it is not optimized for the detection
of sources without taking into account previous information about
the spatial distribution of them. Thus, we used the list of found
sources obtained with ISGRI in the (20-40)\,keV mosaic images (see Figure \ref{mosaic})
as our input catalog. This resulted in GX~339--4 as the only source detected
in the 200--300\,keV energy range (Figure \ref{spi_Hchan}) with a detection
significance of 4.8${\sigma}$.

We combined single revolution SPI
spectra from epochs 1--3, considering that there was no significant
evolution within each revolution (as shown by the relative constancy of the {\it INTEGRAL} and {\it XMM-Newton} light
curves, except for epoch 3 --see below--; Figures \ref{lcurves_xmm} and \ref{lcurves_integral}),
in order to increase the signal to noise ratio. We obtained 3 SPI spectra
in total. The same was done
for the low energy instruments (JEM-X and ISGRI), thus obtaining five
spectra, namely one for each epoch (see Table \ref{tobserv}).
We applied 2$\%$ systematic errors to the JEM-X, ISGRI and SPI spectra. We
restricted our analysis in the energy ranges of $5-20$, $18-200$ and
$23-300$\,keV for the JEM-X, ISGRI and SPI spectral analysis, as
recommended\footnote{For OSA software download, {\tt cookbook} documentation and cross-calibration
issues, we refer to the web page: http://isdc.unige.ch/?Soft+download}.
The SPI and ISGRI spectra were
rebinned at high energies (${\gtrsim}200$\,keV) with the FTOOL
{\tt grppha} procedure to reach the detection level of $2{\sigma}$
per spectral bin.

\subsection{XMM/EPIC-pn} \label{xmm_ins}

The {\it XMM-Newton} Observatory \citep{jansen01aa} includes three
1\,500~cm$^2$ X-ray telescopes each with an {\it European Photon Imaging
Camera} (EPIC; 0.1--15~keV) at the focus. Two of the EPIC imaging
spectrometers use MOS CCDs \citep{turner01aa} and one uses pn CCDs
\citep{struder01aa}. The {\it Reflection Grating Spectrometer};
\citep[RGS; 0.35--2.5~keV,][]{denherder01aa}
are located behind two of the
telescopes. In addition, there is a co-aligned 30\,cm diameter
Optical/UV Monitor telescope \citep[OM,][]{mason01aa},
providing simultaneous coverage with the X-ray instruments.

GX~339--4 was observed by {\it XMM-Newton} for 16.8~ks on 2007 February 19
(hereafter called Obs~1 and coinciding with {\it INTEGRAL} Epoch~2), for 17.8~ks on 2007 March 5
(hereafter called Obs~2 and coinciding with {\it INTEGRAL} Epoch~3) and for 20~ks on
2007 March 30 (hereafter called Obs~3 and coinciding with {\it INTEGRAL} Epoch~5). We refer
to Table \ref{tobserv} for details.

The thin optical blocking filter was used with the EPIC
camera. The EPIC pn camera was operated in burst mode due to the
high count rate of the source (from $\gtrsim$6700~s$^{-1}$ to
$\gtrsim$3000~s$^{-1}$ for Obs~1 to 3, respectively). For the
same reason, the EPIC MOS cameras were not operated. The individual RGS1
and RGS2
CCD chips were read out sequentially. This reduces the frame time from
4.8 to 0.6 seconds
(4.8/8) and consequently the pile-up by almost an order of
magnitude. All the X-ray data products were obtained from the
{\it XMM-Newton} public archive and reduced using the Science Analysis
Software (SAS) version 7.1.0.
In pn burst mode, only one CCD chip (corresponding to a field of
view of 13\farcm6$\times$4\farcm4) is used and the data from that
chip are collapsed into a one-dimensional row (4$\farcm$4) to be
read out at high speed, the second dimension being replaced by
timing information. The duty cycle is only 3$\%$. This allows a time
resolution of 7~$\mu$s, and photon pile-up occurs only for count
rates above 60\,000~s$^{-1}$. Only single and double events
(patterns 0 to 4) were selected. Ancillary response
files were generated using the SAS task {\tt arfgen}. Response
matrices were generated using the SAS task {\tt rmfgen}.
In this paper we do not use RGS spectra because our main aim
is to make a study of the continuum properties of the spectra.

PN Charge Transfer Inneficiency (CTI) rate dependency has been observed
for count rates $>200-300$\,cts/s, i.e.
for very bright sources CTI correction overpredicts the CTI losses. This
can result in an up to 2$\%$ apparent gain shift most visible for spectral
features like edges or lines \footnote{For details see:
http://xmm2.esac.esa.int/docs/documents/CAL-TN-0018.pdf (EPIC
Calibration Status Document), page 4.}. Hereafter,
we applied $2\%$ systematic errors to the EPIC-pn spectra reported
below. We used EPIC ${\rm pn}$ data in the 0.7--10\,keV energy range.

\subsection{Light curves} \label{lc_phenom}

In Figure \ref{lcurves_swift}, we show the SWIFT/BAT and the RXTE/ASM light curve in the
15--50\,keV and 2--12\,keV energy ranges during the entire outburst.
The horizontal lines shown in the Figure indicate the time intervals
(150 ks each, in five observations) over which our average
spectra were obtained. Note that black hole transients usually
begin and end their outbursts in the low/hard state (see \citet{nowak95};
\citet{fender04}; \citet{homanbell05}), and the 2007 outburst
of GX~339--4 is no exception. As can be seen in Figure \ref{lcurves_swift}, the
beginning of the outburst started earlier at high energies (15--50\,keV)
rather than in softer X-rays (2--12\,keV), when observations of epoch 1
were made. The other four
epochs were made during a period when the source spectrum was much
softer. It is interesting to notice the sudden increase of $15\%$ flux (with respect to the maximum value)
of the 15--50\,keV light curve, during the
transition from second to third epoch observations,
possibly associated with changes in the high-energy emission source, as we will discuss in Section \ref{discuss}.

In Figure \ref{lcurves_xmm} we show the XMM/EPIC-pn light curves in the 0.6--10\,keV energy range and
calculated hardness ratio (counts in 2--10\,keV band divided by counts in 0.6--2\,keV) with a time binning of
120\,s. We do not see spectral evolution during the time of each observation due to the constancy
of both the light curves and hardness ratio (except for a small increase in the flux during a short time period
in epoch 3, but of the order of ${\leq}6$\%).

In Figure \ref{lcurves_integral} we show the ISGRI (20--200\,keV) light curves during all the observations.
The source was significantly detected during all the epochs with decreasing flux (except for
epoch 3, with higher flux than for epoch 2). Within every epoch the flux was relatively constant, except for
epoch 3, in which the flux was decreasing with time, with a total flux variation of 70\% around
the mean flux value. In spite of this, we combined all the revolution data to get the spectrum
in this epoch as well (as did for the remainder epochs) in order to get higher signal to noise ratio.

\section{Analysis of spectra} \label{spec_analysis}

We performed fits to the combined JEM-X, ISGRI and, when available, SPI
and XMM/EPIC-pn spectra, for
each of the five epochs (see Table \ref{tobserv}) using XSPEC
\citep{arnaud96} v.11.3. All errors quoted in this work are 90\%
confidence errors, obtained by allowing all variable parameters to
float during the error scan. The hydrogen column density was set to
be free when XMM/EPIC-pn data were available and fixed at
${\rm N}_{\rm H}=0.5{\times}10^{22}$\,${\rm atom}$\,cm$^{-2}$
\citep{dickey90} when only {\it INTEGRAL} data were available.

Our main aim in these fits is to characterize the broad continuum
thanks to the broad {\it XMM-Newton} and {\it INTEGRAL} spectral coverage. To account for
uncertainties in relative instrument calibrations, we fixed JEM-X
multiplicative calibration constant to 1 and let that of ISGRI and SPI
free to vary in the fits for the different data sets as shown in
Table \ref{param_spec}. In the case of using both INTEGRAL and XMM/EPIC-pn spectra, we
fixed  the EPIC-pn multiplicative constant to 1 and let that of JEM-X, ISGRI
and SPI free to vary, in order to account for cross-calibration uncertainties
as well \footnote{We restricted the values of the multiplicative constants to
be $1,{\approx}1{\pm}20\%,1{\pm}30\%,1{\pm}60\%$ for XMM/EPIC-pn,JEM-X,
ISGRI and SPI relative to XMM/EPIC-pn in order
to obtain reliable fits. When XMM/EPIC-pn data was not available, the same ratio
between the constants was preserved.}.
The presence of an XMM/EPIC-pn instrumental line was clear in the spectra
of epochs 2 and 3 and we added a gaussian emission line centered at $2.28$\,keV and
$2.25{\pm}{0.03}$\,keV, respectively. For epoch 5 two absorption instrumental
lines appeared, centered at $1.82$\,keV and $2.14$\,keV, respectively.
As mentioned in the {\it XMM-Newton} analysis of GRO~J1655--40 \citep{diaz07};
where these features were present as well,
structured residuals near 2.3\,keV are probably due to an incorrect
instrumental modeling of the Au mirror edges, whilst those near 1.8\,keV are probably due
to an incorrect modeling of the Si absorption in the CCD detectors.

\subsection{Fits of joint XMM/EPIC-pn and INTEGRAL spectra with phenomenological models} \label{spec_phenom}

We performed preliminary fits to the spectra of every single epoch with the phenomenological model
consisting of a multicolor disk black body ({\tt diskbb} in XSPEC) of \citet{mitsuda84} plus a
powerlaw convolved by absorption at low energy in order to describe the high-energy emission.
In none of the observations this model provided a good fit to the data
(${\chi}^{2}_{\nu}=46,3.05,4.2,1.8,3.3$ for ${\nu}=96,150,154,46,108$
for epochs 1, 2, 3, 4 and 5, respectively).

In epoch 1 the situation improved dramatically (${\chi}^{2}_{\nu}=2.76$, ${\nu}=94$)
when a high-energy cut-off was included in the model (i.e. {\tt constant*phabs(diskbb + powerlaw)highecut}; ${\rm E}_{\rm c}{\approx}70$\,keV).
Nevertheless, some positive and negative residuals still remained at 6--10\,keV and 10--20\,keV,
in the form of a steepening of the spectrum and of an edge, respectively,
indicating the likely presence of a broad ${\rm Fe}$\,${\rm K}_{\alpha}$ line. We included
a broad ${\rm Fe}$ gaussian line centered at ${\rm E}_{\rm Fe}=6.4-6.97$\,keV, getting the final statistics of
${\chi}^{2}_{\nu}=1.4$ (${\nu}=91$). With the model {\tt constant*phabs(diskbb+gaussian+powerlaw)highecut},
the final values obtained for the photon index and the folding energy are of ${\Gamma}=1.46^{+0.03}_{-0.02}$ and
$E=66.4^{+0.9}_{-1.1}$\,keV, respectively. These values resemble those found by \citet{belloni06} during the HIMS
of the 2004 outburst.

In epoch 2 low-energy positive residuals in the form of an excess near 1\,keV were
detected in the XMM/EPIC-pn spectrum and the fit greatly improved when considered (${\chi}^{2}_{\nu}=1.9$, ${\nu}=144$).
The obtained equivalent width is $W_{1\,keV}=11.6{\pm}2.1$\,eV.
This feature is detected in a number of X-ray binaries and has been previously modeled
either as an emission line, or as an edge, and its nature is unclear
(e.g. \citet{kuulkers97}; \citet{sidoli01}; \citet{boirin03}, \citet{diaz07}). However, since this has not been detected
before in GX~339--4 we think that this line probably is an instrumental effect due to incorrect modeling of
${\rm Ne}$\,${\rm IX}$ and ${\rm Ne}$\,${\rm X}$ and ${\rm Fe}$\,${\rm L}$ in the CCD detector.

In epoch 3 positive and negative residuals appeared, centered at ${\approx}6-10$\,keV and
${\approx}10-20$\,keV, respectively (see Figure \ref{skewed_Fe}).
These residuals are compatible with a broad and skewed ${\rm Fe}$\,${\rm K}_{\alpha}$ line and the respective ${\rm Fe}$ edge.
As in epoch 1, we added a gaussian line centered at ${\rm E}_{\rm Fe}=6.4-6.97$\,keV and the fit improved (${\chi}^{2}_{\nu}=3.3$, ${\nu}=146$), but
some residuals in the red wing of the ${\rm Fe}$ line (3--5\,keV) still remained. These residuals point out to the ${\rm Fe}$\,${\rm K}_{\alpha}$ line
having a relativistic origin (i.e. originated very close to the black hole). Thus, we substituted the gaussian component by a {\tt laor} \citep{laor91}
model, which includes general relativity effects in the modeling of the X-ray emission in the inner boundaries of a rotating black hole.
The parameters of this model are the line energy $E$, the disk emissivity index $q$
(where the emissivity is assumed to have a power-law form of $J(r){\propto}r^{-q}$; where $q=3$ is expected for a standard disk), the inner
radius of the line emission region in units of $GM/c^2$ (with a lower limit of 1.235\,$R_{g}$ for a maximally rotating black hole), the outer
line emission radius in units of $GM/c^2$ (fixed to the fiducial value of 100\,$R_{g}$), the disk inclination, and the line normalization.
With this model, we obtained significant
better statistics (${\chi}^{2}_{\nu}=2.7$, ${\nu}=143$) and flat residuals in the 3--5\,keV energy range, where the relativistic effects of the ${\rm Fe}$
complex are expected to appear \footnote{Whilst in epoch 1 there are residuals compatible with the broad $Fe$ line, we can not test
if its origin is relativistic, due to the JEM-X lower energy limit of 5\,keV, where the relativistic red wing is expected to appear. Thus, complex models
dealing with the sophistication of the red wing line (as {\tt laor}), can not be applied to the data of epoch 1.}.
The inner radius of the disk, the emissivity index, the disk inclination and the normalization
were free to vary in the fit. We allowed the value of the inclination to vary in the range 10$^{\circ}$--60$^{\circ}$.
The value obtained for the line energy is very high ($6.83{\pm}0.14$\,keV), indicating a very ionized medium.
The obtained value for the emissivity index is rather steep ($q=5.2^{+0.5}_{-1.0}$), being
close to the value found in the VH state ($q=4.8-6$ by \citet{miller04a}).
The obtained value for the disk inclination is $i=35^{+4}_{-7}$$^{\circ}$.
High values for the emissivity index indicate that the primary source is very close to the black hole. Steep emissivity indices
(${\approx}7$) have been observed from a number of Seyfert galaxies (e.g. \citet{fabian04}; \citet{fabian05}).
The inner radius obtained was rather low ($r_{in}=2.11{\pm}0.11$\,$R_{g}$), thus being
clearly different from 6\,$R_{g}$ (expected value for a non-rotating Schwarzschild black hole) and close to the value found
by \citet{reis08} ($r_{in}=2-2.1$\,$R_{g}$).
The presence of negative residuals at 10\,keV led us to consider the effects of a smoothed absorption of
the $Fe$ ions in the inner disk. We included a smoothed absorption edge ({\tt smedge} in XSPEC) and the
fit improved, getting the final statistics of ${\chi}^{2}_{\nu}=1.3$ (${\nu}=141$). Relativistic smearing is expected
to appear in the inner parts of the accreting disk and, with $Fe$ line, accounts phenomenologically for reflection.
This resulted in an edge energy of $E_{\rm smedge}=8.53{\pm}0.20$\,keV, compatible with
He-like configuration for $Fe$ and
${\tau}=1.09^{+0.15}_{-0.11}$, with a smeared edge width frozen to $W_{\rm smedge}=5$\,keV (close to the value found by
\citet{reis08} in the VH state; i.e. $W_{\rm smedge}=4.5^ {+0.5}_{-2.0}$\,keV).

In epoch 4 some residuals remained in the form of a smeared edge in the 10--20\,keV
energy range. When considered (i.e. model {\tt constant*smedge*phabs(diskbb + powerlaw)}), the fit improved (${\chi}^{2}_{\nu}=1.2$, ${\nu}=44$),
meaning an F-test probability of 1.337E-04 that the improvement was made by chance. The value obtained for the threshold energy  and
the maximum absorption factor at threshold are $E_{\rm smedge}=9.53^{+0.5}_{-0.6}$\,keV and ${\tau}=1.6{\pm}0.5$, respectively, compatible with
H-like configuration for $Fe$.

Finally, in epoch 5, residuals in the form of an excess at ${\gtrsim}50$\,keV and a smeared edge at
7--10\,keV (${\chi}^{2}_{\nu}=3.3$, ${\nu}=108$) were present. In the residuals there was an emission line like in epoch 2
and we included an emission gaussian line centered at ${\approx}1$\,keV (${\chi}^{2}_{\nu}=2.4$, ${\nu}=105$). The equivalent width
obtained was $W_{1\,keV}=29{\pm}5$\,eV, thus higher than in epoch 2.
When adding the smoothed
edge (i.e. model {\tt constant*smedge*phabs(diskbb + powerlaw + gaussian)}) the fit greatly improved
(${\chi}^{2}_{\nu}=1.3$, ${\nu}=104$). The obtained values for both the threshold energy and maximum absorption factor at threshold
are $E_{\rm smedge}=9.22{\pm}0.25$\,keV and ${\tau}=3.0{\pm}0.5$, respectively, the former compatible with
H-like configuration for $Fe$ \footnote{The edge
for neutral iron is at 7.1 keV, for He-like iron at 8.8 keV, and for
H-like iron at 9.3 keV.}. The value for the absorption factor at threshold is very high and would indicate that it is not due to
the presence of an absorber, rather being due to reflection effects.
The excess above 50\,keV would indicate an important source of Comptonization by non-thermal particles, as occurring in epoch 1, as shown below.

The values obtained for the best fit parameters with the best phenomenological
fit are shown in Table \ref{param_spec} and the spectra with the best fit results are shown in Figures
\ref{fit_spec1} and \ref{fit_spec2}. In Table \ref{param_over} we summarize the
values for the photon indices of the powerlaw (analyzed in this Section) and un-absorbed
luminosities of both the powerlaw and the disk (assuming a distance to the source of 8.5\,kpc).

\subsection{State classification and related behavior}   \label{state_class}

The main features of the spectrum of epoch 1 are a rather flat photon index (${\Gamma}=1.46^{+0.03}_{-0.02}$) and
the clear presence of a high-energy cut-off at $66.4^{+0.9}_{-1.1}$\,keV. The value found for the cut-off is
very close to the value reported by \citet{belloni06} ($E_{c}=70^{+10}_{-8}$\,keV) during HIMS, although the value found
for the photon index in their case was clearly steeper (${\Gamma}=1.92{\pm}0.05$). We conclude that the
spectrum of epoch 1 corresponds in luminosity (\citet{belloni97}, \citet{fender04}, \citet{homanbell05}) and
spectral characteristics to the HIMS.
During epochs 2 and 3 the spectra are characterized by
a steep high-energy emission (${\Gamma}{\approx}2.33{\pm}0.02,2.659^{+0.004}_{-0.01}$
for epochs 2 and 3, respectively). In the classification scheme of
\citet{homanbell05}, both correspond to the SIMS.
The value of the photon index from epoch 2 resembles those
reported previously by \citet{nespoli03} (${\Gamma}=2.44{\pm}0.10$) and \citet{belloni06} (${\Gamma}=2.3$)
during SIMS of GX~339--4 as well. The inner disk temperatures found are $0.891{\pm}0.003$\,keV and $0.852^{0.005}_{-0.008}$\,keV,
thus resembling the values found by \citet{malzac06} and \citet{cadollebel05} (i.e. $1.2{\pm}0.2$\,keV) for Cyg~X--1 in Intermediate states as well.
Observations of GX~339--4 during the 2004 outburst by \cite{miller04a} during the VH state
show the same photon index value for the high-energy emission (i.e. ${\Gamma}=2.61^{+0.09}_{-0.01}$) as us for epoch 3, accompanied
by a detection of a relativistic $Fe$ line, as well. Indeed, in the most recent state prescription \citep{homanbell05},
the VH state is the same as the SIMS.

The spectrum during epochs 4 and 5 is characterized by a
steep high-energy emission (${\Gamma}=2.39{\pm}0.06,2.65{\pm}0.02$). As can be seen in Figure \ref{lcurves_xmm}
the hardness ratio (defined as HR=(2-10)\,keV)/(0.2-2)\,keV) of the light curves are very
soft in epochs 4 and 5. The inner disk temperatures found for these epochs are $0.75^{+0.07}_{-0.06}$\,keV and $0.698{\pm}0.003$\,keV,
respectively, thus resembling the values found in the HS state
for Cyg X-1 (i.e. 0.6\,keV \citet{gierlinski99}, \citet{frontera01}). The softness, the inner disk temperatures, the values for the photon
index and the high value for the disk normalization
component suggest that the source in those epochs is in the
high/soft state, considering the classification scheme of \citet{homanbell05}. The spectral evolution
is presented in Figure \ref{spec_state}.

As explained above, our observations of GX~339--4 cover the spectral
evolution from the HIMS to high/soft state, passing through the SIMS.
As shown in Section \ref{spec_phenom} and in Table \ref{param_over}, this
spectral evolution involves very significant spectral changes which are strongly correlated. The changes
in the spectral shape are strongly correlated with
the ratio of the powerlaw to the disk luminosity.
In the first epoch there was almost no disk contribution in the spectrum. It showed a cut-off
at ${\rm E}_{\rm c}=66.4^{+0.9}_{-1.1}$\,keV in the powerlaw. The cut-off disappeared in the second epoch
and the powerlaw emission decreased notably, being just $1/7$ of the disk luminosity.
In the third epoch the spectrum hardened again considerably (the powerlaw luminosity being 1.7 times
higher than the disk luminosity, the latter decreased by $50\%$ with respect to the second epoch).
The total luminosity increased by 50\% in the transition from epoch 1 to 2 and remained more or less
unchanged during epochs 2 and 3, while decreasing in epoch 4 and 5 (again decreased by $50\%$).
The luminosities obtained for all the epochs
were within the range of $20-50\%$ the Eddington luminosity
(assuming the compact object being a black hole of $6{\rm M}_{\odot}$).

\section{The high-energy excess} \label{spec_excess}

During the LH state of the GX 339--4 outburst occurring in 1991, a high-energy excess (above 200\,keV) was
observed with OSSE (\citet{johnson93}, \citet{wardzinski02}). In 2004, during the increasing phase
of the 2004 outburst, \citet{joinet06} observed a similar feature with SPI when GX 339--4 was in its
canonical LH state. Similar features have been recently reported for other black hole transients in LH
states observed during the decreasing phase of their outbursts (\citet{kalemci06}, \citet{kalemci05}). It
is also more commonly associated with state transitions \citep{malzac06} and with soft states \citep{gierlinski99}.

Such a hard tail is ussually attributed to the presence of a small fraction of non-thermal
electrons in the hot Comptonizing plasma.
In the HIMS of our observations (epoch 1), GX 339--4 shows a highly significant cut-off
at $66.4^{+0.9}_{-1.1}$\,keV. This indicates that soft photons are Comptonized by a thermal electron
population with a temperature $kT_{e}$ that is related to the cut-off energy. Both for the HIMS (epoch 1) and
SIMS (epochs 2 and 3) non-negligible values of ${\ell}_{nth}/{\ell}_{h}$ were found (as shown below in Section \ref{spec_eqpair}).

In order to investigate further the possible presence of a non-thermal component during the HIMS and SIMS,
IBIS and SPI spectra have been fit with the COMPPS model of \citet{poutanen96} (see Table \ref{fit_compps_param}).
In this thermal Compton model, the spectrum is computed for a homogeneus spherical
hot corona, inside which blackbody photons are injected and then upscattered by hot Maxwellian electrons. The reflected spectrum is
smeared out by rotation of the disk due to special and general relativistic effects using {\tt diskline}-type kernel.
As in the {\tt comptt} model \citep{titarchuk94},
the corona is parametrized by its electron temperature, $T_{e}$, and the radial Thompson optical depth, ${\tau}=n_{e}{\sigma}_{T}H$,
where $n_{e}$ is the electron density, ${\sigma}_{T}$ is the Thompson cross section and $H$ the radius of the sphere.
Using this thermal Comptonization model, some residuals are present at high-energy, especially in the
spectrum of epoch 1. In order to mimic the presence of a non/thermal component, we added a powerlaw
to the pure Comptonization model (see Figure \ref{fit_compps}). This led to an improvement of the ${\chi}^{2}$ that is
significant for epoch 1 (see Table \ref{fit_compps_param}). The F-test probability that this improvement was made
by chance is $p=6.461E-02$ for epoch 1. On the contrary, because of the low statistics
in epochs 2 and 3, adding a powerlaw to the thermal Comptonization model is not required. However, we notice that the
electron temperatures obtained with the thermal Compton plus powerlaw model are rather close to the values obtained with
EQPAIR fits for all the epochs.

\section{Fits of joint XMM/EPIC-pn and INTEGRAL spectra with the hybrid thermal/non-thermal Comptonization EQPAIR model} \label{spec_eqpair}

\subsection{The model}

We saw in the previous Section that a high-energy excess is visible in the spectra. Since this high-energy excess
can not be well described by thermal Comptonization, we go into more sophisticated models containing
a hybrid distribution of thermal/non-thermal particles. From the variety of
Comptonization models available in the literature, we have chosen the hybrid thermal/non-thermal Comptonization EQPAIR model \citep{coppi99},
and relativistic line emission and disk reflection. The best-fit values for the parameters for all the epochs are shown
in Table \ref{fit_eqpair_param}. Because the presence of an instrumental line at ${\approx}1$\,keV in the XMM/EPIC-pn spectra of epochs 2, 3 and 5
was analyzed in Section \ref{spec_phenom}, this will not be discussed further.

In the EQPAIR model, emission of the disk/corona system is modeled by a spherical hot plasma cloud with
continuous acceleration of electrons illuminated by soft photons from the accretion disk. At high-energies
the distribution of electrons is non-thermal, but at low energies a Maxwellian distribution with temperature
$kT_{e}$ is established.

The disk spectrum incident in the plasma is modeled as coming from a pseudo-Newtonian accretion disk
(${\tt diskpn}$ in XSPEC) extending from $R_{out}=100$\,$R_{g}$ down to the minimum stable orbit
$R_{out}=6$\,$R_{g}$. Its spectral shape is then characterized by the maximum color temperature of the disk,
$kT_{pn}$. Previous observations of Cyg X-1 with X-ray telescopes indicate temperatures ranging from 0.1\,keV
in the LH state up to 0.6\,keV in the HS state (\citet{gierlinski99}, \citet{frontera01}).

The model (EQPAIR) takes into account angle dependence, Compton
scattering (up to multiple orders), photon pair production, pair
annihilation, bremsstrahlung, as well as reflection from a cold disk.
This model includes ionized Compton reflection (as the {\tt pexriv} model in XPSEC; \citet{magdziarz95}).
The reflection component is smeared out by rotation of the disk due to special and general relativistic
effects using {\tt diskline}-type kernel to relativistic motion in the disk
(as in the {\tt diskline} model in XSPEC; \citet{fabian89}). We used the
LAOR model \citep{laor91} to model the relativistic iron line emission, with the
emissivity index (${\beta}$) free and tied to the opposite value of that of the EQPAIR.
The disk reflection component is calculated for neutral material with standard
abundances, unless otherwise noted. We asumed free inclination and inner disk radius in the range of $10^{\circ}-60^{\circ}$
and $2-6$\,$R_{g}$. The outer disk radius was fixed to 100\,$R_{g}$.

The EQPAIR model provides the injection of a non-thermal electron distribution
with Lorentz factors between ${\Gamma}_{min}$ and ${\Gamma}_{max}$ and
a powerlaw spectral index ${\Gamma}_{inj}$.
The system is characterized by the power (i.e. luminosity)
$L_{i}$ supplied by its different components. We express each of them
dimensionlessly as a compactness parameter,
${\ell}_{i}=L_{i}{\sigma}_{\rm T}/(R m_{e}c^{3})$,
where $R$ is the characteristic dimension and ${\sigma}_{\rm T}$
the Thompson cross-section of the plasma. Thus, ${\ell}_{s}$, ${\ell}_{th}$,
${\ell}_{nth}$ and ${\ell}_{h}={\ell}_{th}+{\ell}_{nth}$ correspond to
the power in a soft disk entering the plasma, thermal electron heating,
electron acceleration and the total power supplied to the plasma.
The total number of electrons (not including ${\rm e}^{+}{\rm e}^{-}$ pairs)
is determined by ${\tau}_{\rm T}$,
the corresponding Thompson optical depth, measured from the center
to the surface of the scattering region. If we consider injection from pairs
${\rm e}^{+}{\rm e}^{-}$, then the total optical depth of the thermalized
scattering electrons/pairs is expected to be ${\tau}_{\rm T}{\geq}{\tau}_{\rm P}$.

In general, the spectral shape is insensitive to the exact value of the compactness, but
it depens strongly on the compactness ratios (${\ell}_{h}/{\ell}_{s}$ and  ${\ell}_{nth}/{\ell}_{h}$).
Thus, we froze ${\ell}_{s}$ to a fiducial value (${\ell}_{s}=10$), as commonly
reported for other sources with similar characteristics (e.g. \citet{ibragimov05}). In the
fits reported below, we fit the data with a powerlaw distributed injection of electrons and compare
with the results obtained with a mono-energetic distributed injection of them as well. The former
distribution is expected in the case of shock acceleration of particles, while the second
could be achieved in reconnection events that are expected to power the corona \citep{galeev79}.

\subsection{Fits to the data}

For the first epoch of our observations, due to the low disk contribution, we froze the
disk temperature to a fiducial value of $kT_{pn}=300$\,eV, as an intermediate value
between LH and HS values found by \citet{gierlinski99} and \citet{frontera01} for Cyg~X--1. The relativistic
Fe disk line emission was significant (with a chance probability of 4.823E-05).
The most relevant factor is the inclination
angle of the reflecting material, clearly favouring high values. We obtained worse residuals
and statistics (${\chi}^{2}_{\nu}=1.8$, ${\nu}=82$) for the case of $i=30^{\circ}$ with
respect to the case of $i=50^{\circ}$ (${\chi}^{2}_{\nu}=1.0$, ${\nu}=82$).
Since this value is in conflict with the value obtained in Section \ref{spec_phenom} and the
values obtained from fitting the X-ray data in the literature, we will adopt $i=30^{\circ}$ in the fits
of the remainder epochs \footnote{We repeat the same analysis by considering $i=50^{\circ}$ for
epochs 2, 3, 4 and 5 and the results do not change significantly with respect to the case
$i=30^{\circ}$.}. High values for the ionization are preferred by the data, with an
improvement of ${\Delta}{\chi}_{\nu}^{2}=0.5$ (for 82 d.o.f) with respect to the neutral case.
The spectral cut-off already noticed in Section \ref{spec_phenom} can be
modeled here by Comptonization of thermal distributed particles and reflection from a
cold disk. As shown in \citet{petrucci01}, with an electron temperature of $kT_{e}=27.5{\pm}1.2$\,keV
and an optical depth of ${\tau}=2.39^{+0.15}_{-0.18}$, it is possible to reproduce the
spectral cut-off at $66.4^{+0.9}_{-1.1}$\,keV. The spatial distribution of the
Comptonizing particles is compact (${\ell}_{h}/{\ell}_{s}=3.9^{+0.6}_{-0.3}$) and mildly non-thermal
(${\ell}_{nth}/{\ell}_{h}=0.40^{+0.15}_{-0.03}$). The high-energy distribution is well
fit with a powerlaw injection of non-thermal electrons with relatively low photon
index (${\Gamma}_{inj}=1.80^{+0.07}_{-0.05}$) with Lorentz factors within the range
1.3--100 (as considered in the remainder epochs as well). This issue means the clear presence of non-thermal
particles in the plasma. When fitting with a mono-energetic distribution of electrons
with a Lorentz factor of ${\Gamma}=5$, the fit slightly worsened (${\chi}^{2}_{\nu}=1.1$, ${\nu}=83$
and worse description of the highest energy emission) with respect to the previous fit
(i.e. ${\chi}^{2}_{\nu}=1.0$, ${\nu}=82$).
Albeit not significant, the spectrum seems to be better described by a powerlaw
injection of non-thermal electrons. Clearly, higher energy data are needed in order to
disentangle these models.

In the second epoch, XMM/EPIC-pn data allowed us to constrain the disk temperature
($kT_{pn}=897^{+1.4}_{-1.3}$\,eV). The relativistic Fe disk line emission was found to be
zero (no improvement of the statistics at all, when considered). The data preferred a neutral reflecting disk
(with ${\Delta}{\chi}^{2}=0.15$ of improvement for 142 dof) and the final statistics is
${\chi}^{2}_{\nu}=1.7$ (${\nu}=142$). The statistics is poor and the disk temperature
very high, which would indicate that EQPAIR model is not adequate enough to describe the softest
part of the spectrum of this epoch \footnote{As reported in \citet{malzac06} and \citet{cadollebel05},
such high inner temperatures are not realistic for Cyg~X--1. \citet{malzac06} included an additional
warm Comptonization model to the EQPAIR model to describe the soft part of the spectrum
during the Intermediate state finding very good agreement with the data. However, this kind
of work is out of the scope of this paper.}.
Nevertheless, the high energy spectrum is well described
by a purely non-thermal dominated distribution of particles (${\ell}_{nth}/{\ell}_{h}=0.9{\pm}0.1$).
However, the photon index of the powerlaw injection distribution of the Comptonizing electrons
is very steep (${\Gamma}_{inj}=2.87^{+0.05}_{-0.06}$), which indicates the presence of mildly relativistic electrons.
Both the coronal compactness and opacity were found to be very low
(${\ell}_{h}/{\ell}_{s}=0.05^{+0.003}_{-0.01}$ and ${\tau}_{p}<0.02$) \citep{nowak02}.
Albeit the spectrum does not show significant relativistic smearing, the reflection covering factor was
found to be significant (${\Omega}/2{\pi}=0.40_{-0.04}^{+0.3}$). We obtained the same quality fit when
considering a mono-energetic distribution of electrons with a Lorentz factor of
${\Gamma}=5$ (${\chi}^{2}_{\nu}=1.7$, ${\nu}=143$).

In the third epoch the disk temperature was found to be $kT_{pn}=704{\pm}2$\,eV, thus resembling the
values found in soft states for Cyg X-1 (\citet{gierlinski99}, \citet{frontera01}).
Albeit in the phenomenological fits reported in Section \ref{spec_phenom} the presence of a relativistic
iron line was clear in the residuals, we notice the lack of its significance in this model (just a chance probability of
1.151E-04 compared with 1.040E-09 from the phenomenological fits). This issue can be
understood by the fact that the {\tt pexriv} model (which is incorporated in EQPAIR to account for reflection)
is not a proper description of the reflection occurring
in the inner parts of an accretion disk, since it does not include the Compton scattering (and consequent blurring
in energy) that must occur. The statistics obtained
is ${\chi}^{2}_{\nu}=1.5$ (${\nu}=138$) and the
high-energy spectrum is well described taking into account thermal and non-thermal distributed particles
in the plasma, by the same amount, as occurring in epoch 1. The photon index of the powerlaw distribution
of non-thermal injected particles is very steep (${\Gamma}_{inj}=3.42^{+0.03}_{-0.04}$), meaning a mildly relativistic
population of non-thermal electrons. Both the coronal compactness and the opacity
(${\ell}_{h}/{\ell}_{s}=0.28^{+0.03}_{-0.01}$ and ${\tau}_{p}=1.43^{+0.03}_{-0.06}$) are as found in \citet{delsanto08}.
The relativistic smearing in this spectrum is important, meaning that reflection probably occurs in the inner
regions of the accretion disk. High values for the reflection covering factor were favored and we froze this value
(${\Omega}/2{\pi}=1$).
We considered a mono-energetic injection of electrons case as well (${\Gamma}=5$) and we obtained clearly worse agreement with
the data (${\chi}^{2}_{\nu}=1.9$, ${\nu}=139$) and with a large discrepancy of the highest energy bins. In this
epoch a powerlaw injection of electrons is clearly favored against the mono-energetic injection scenario.

The results obtained for the fits of epoch 4 resemble those obtained for epoch 3.
The maximum disk temperature was frozen to a fiducial value of
500\,eV, for the same reason as well. When considering a powerlaw injection of non-thermal electrons, the fit statistics
obtained is ${\chi}^{2}_{\nu}=1.5$ (${\nu}=44$). The corona is relatively compact, mildly non-thermal and relativistic
smearing is important, thus giving a very high value of the reflection covering factor (${\Omega}/2{\pi}=1$), as
in epoch 3. Again a mono-energetic injection of electrons is a very poor description of the data (${\chi}^{2}_{\nu}=4.5$; ${\nu}=45$)
with a large discrepancy of the highest energy bins. It is worthy to notice as well that in this case the iron line emission
(modeled here as a LAOR component)
was not significant in the data and even worsened the fit when considered (by ${\Delta}{\chi}_{\nu}^{2}=0.3,0.2$ for cases
of $i=30^{\circ}$ and $i=50^{\circ}$, respectively).

For epoch 5 we could determine the disk temperature ($kT_{pn}=550{\pm}5$\,eV). The relativistic line was significant
(with a chance probability of 1.029E-06) and the reflection covering factor very
high (${\Omega}/2{\pi}=0.72^{+0.16}_{-0.10}$). The fit statistics was ${\chi}^{2}_{\nu}=1.6$ (${\nu}=99$). As in epochs 1,
3 and 4, mono-energetic injection of non-thermal electrons is not a good description of the data, due to the worse
statistics (${\chi}^{2}_{\nu}=1.7$, ${\nu}=100$) and discrepancy of the high-energy channels. The observed temperature of the
disk is cooler (HS state) than in epoch 3 (SIMS state). This fact is accompanied by the increase of the compacticity
for the latter and would indicate that the corona becomes more compact as the disk temperature increases.

Spectra and models of the five different periods have been plotted in Figure \ref{spec_state}.

\section{Discussion and conclusions} \label{discuss}

During our observations, we detect spectral evolution from the HIMS to the HS state, passing through SIMS.
We performed phenomenological and more physical motivated fits to the data and found that during the HIMS
the spectral cut-off at $66.4^{+0.9}_{-1.1}$\,keV is due to the thermal kinetic distribution of electrons in the plasma.
For the SIMS and HS states we do not find a significant cut-off in the data but applying analysis with
Comptonization models (EQPAIR and COMPPS) we detect a high-energy tail in all the epochs that can be understood
as evidence of a non-thermal distribution of particles in the plasma. The detection of the non-thermal component
in GX~339--4 in the LH state was done previously by \citet{joinet06} and in the HIMS by \citet{delsanto08}.
We thus confirm the detection
of the non-thermal component in the SIMS as well (as previously done by \citet{malzac06} for Cyg~X--1).

The results obtained by applying EQPAIR fits to the data indicate a high value for the coronal compactness for epoch 1,
but within the range of values found in the literature. For epochs 3, 4 and 5 this value is high as well (when compared
to that obtained in epoch 2). We thus confirm the correlation between coronal compactness and covering fraction of the cold
reflecting material by \citet{nowak02} for epochs 2 to 5. The high value of the coronal compactness found for epoch 1 (HIMS)
would indicate that the Comptonizing high-energy source is compact in size. This would be in agreement with the proposed
scenario of \citet{markoff05}, in which the base of the jet could be the source of the Comptonizing elecrons.
The fact that we are detecting the thermal cut-off would be consistent with the detection of the coronal emission as well.
However, for epoch 2 (SIMS), the values for both the coronal compactness and opacity found
are extremely low. Furthermore, the kinetic temperature found for the thermal electrons in the corona
is very high (and close to the high-energy limit indeed). We understand these as issues indicative of the absence of
coronal emission during this epoch. During epochs 3 to 5 (SIMS to HS), both the coronal compactness and opacity
increase again (accompanied with the significant detection of a relativistic line in epoch 3), thus indicating re-appearance of
the corona after epoch 2.

The results reported above are supported by the different fits we have done with the hybrid thermal Comptonization
(EQPAIR) model. We fit the data with a powerlaw distributed injection of electrons and compared
with the results obtained with a mono-energetic distributed injection of them as well. The former
distribution is expected in the case of shock acceleration of particles, while the second
could be achieved in reconnection events that are expected to power the corona \citep{galeev79}. We found that the first model
is better than the second for epochs 1, 3, 4 and 5. This is indicative of a corona of particles distributed at different
speeds being the source of the high-energy emission. However, for epoch 2, albeit the first proposed scenario is not
discarded, and contrary to the remainder epochs, a mono-energetic distribution of particles is a good description
of the spectrum. It seems that magnetic reconnection events are driving the high-energy emission in this epoch.

Thus, we conclude that we detect spectral evolution in our data compatible with disappearance of a part \footnote{Since the model still requires a high-energy component.}
of the corona in epoch 2 (SIMS). This was followed by its re-appearance in epoch 3 (SIMS)
and maintained in epochs 4 and 5. Giving strength to this
interpretation is the fact that \citet{corbel07} detected a series of plasma ejection events during 4--18 of
February (2007) in radio, just previously to our observations of epoch 2. Also, the sudden increase in flux in the 15--50\,keV
of the SWIFT/BAT light curve (Figure \ref{lcurves_swift}) of $15\%$ could be related to changes occurring in the source of the
high-energy emission during the transition from epochs 2 to 3.
The possible disappearance of the corona during epoch 2 resembles what claimed by
\citet{rodriguez08} in the case of GRS~1915+105. This behavior could be understood
as the fact that the ejected medium is the coronal material responsible for the hard X-ray emission.
The spectra of epochs 1, 3, 4 and 5 show a significant fraction of non-thermal particles as well, indicating that
it could be due to other processes apart from thermal Comptonization. For example, synchrotron or self-synchrotron
emission (\citet{markoff03},\citet{markoff05}) occurring at the base of a jet.

\acknowledgments

MCG acknowledges very useful discussion with J. Malzac. This work is based on observations
made with {\it INTEGRAL}, an ESA science mission with
instruments and science data centre funded by ESA member states and
with the participation of Russia and the USA and on observations with {\it XMM-Newton},
an ESA science mission with instruments and contributions directly funded by ESA
member states and the USA (NASA). We thank to K. Arnaud for providing part of
the eqpair code used in this work. We also thank E. Jourdain for the valuable discussions
regarding SPI data analysis and the anonymous referee for the very useful comments, which improved greatly the quality of the paper.
JMM aknowledges funding from NASA through the INTEGRAL Guest Observer program.
MCG was a MEC funded PhD student during the main work of this paper, supported under grants
PNE2003-04352+ESP2005-07714-C03-03. DS acknowledges a STFC Advanced Fellowship as well as
support through the NASA Guest Observer program. We also acknowledge the Swift/BAT team
for the Swift/BAT transient monitor results.

redpajama_set_name: RedPajamaArXiv


text:
Власовка — хутор в Тарасовском районе Ростовской области.

Входит в состав Зеленовского сельского поселения.

География
На хуторе имеется одна улица — Дачная.

Население

Достопримечательности
Примерно в 1800 метрах от села Власовка находится древнее поселение бронзового века Власовка-1. Поселение относится к этнокультурному объединению эпохи поздней бронзы (XVIII—XII век до нашей эры). Срубная культура, была распространена в степной и лесостепной полосах Восточной Европы между Днепром и Уралом.

На месте раскопок было найдено углубление под древнее полуземляночное строение, предметы была и охоты. Культурный слой раскопок представлен материалами:
куски лепной керамики; предметы из глины и камня; кости домашних животных (коза, бык, лошадь, овца); части амфор салтово-маяцкой культуры (VIII—X век нашей эры); каменный наконечник стрелы энеолитического периода (относится к раннему периоду посещения людей).

Литература
 Цыбрий Т. В. Поселение Ягодинка 2 и некоторые вопросы домостроительства на Нижнем Дону в эпоху поздней бронзы. Санкт-Петербург. 2013. Институт истории материальной культуры РАН.
 Цыбрий A. B., Шеф A. B. Раскопки поселения эпохи поздней бронзы Власовка 1 в Тарасовском районе Ростовской области // сб. Археологические записки. Ростов-на-Дону, 2002. Вып. 2. — С 161—168.
 Цыбрий Андрей Витальевич. Отчёт об охранных археологических исследованиях поселения Власовка 1 в Тарасовском районе Ростовской области в 2001 году / Ростов-на-Дону, 2002. Архив ДАО. Р-1. № 48/П.

Примечания

Ссылки
 Власовка (хутор)

Населённые пункты Тарасовского района

redpajama_set_name: RedPajamaWikipedia


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Flash Flood Video from DataPath Offices Makes National News | DataPath, Inc.
On Wednesday, March 30, the Little Rock area was hit by a flash flood due to heavy rains. Some estimates show that central Arkansas received four inches of rain over a two-hour period. The torrential rain affected many areas around the city as it overwhelmed drainage systems, creeks, and other waterways.
At the DataPath offices at 1601 Westpark Drive, the deluge caused flash flooding that submerged employees' vehicles and created a chaotic scene as dumpsters floated through the swiftly moving waters and crashed into parked cars. DataPath employees rushed to move their vehicles and assist others during this frantic event. Many employees watched the action from the rear of the building and the company's social media analyst, Jessi Hardy, captured some video and posted it to Twitter. The video was quickly picked up by local and national news services, such as The Weather Channel, The Huffington Post and USA Today.
The clip shows a green recycling dumpster being swept along a fence line through the current, as it heads toward a parked truck. One associate implores others to help out the truck owner. The frenzy was captured perfectly by Ms. Hardy.
DataPath is grateful for the teamwork shown by its employees and also prays that all those affected by this severe weather event are okay.


text:
Margaret Thatcher casts a long shadow over theatre and the arts
Michael Billington
She had little time for culture – and once hailed Andrew Lloyd Webber as a great British export. But Thatcher dominated playwrights' imaginations, along with so much else
Ball-breaking ... Haydn Gwynne as Margaret Thatcher in The Audience. Photograph: Johan Persson
Mon 8 Apr 2013 11.44 EDT
Margaret Thatcher may not have cared passionately about the arts, but she left her emphatic mark upon them. Under her watch from 1979 to 1990 we saw a shift away from public subsidy to corporate sponsorship, a transformation of the Arts Council from an independent agency to an instrument of government, and the growth of a siege mentality in arts organisations. While a lot of ground was retrieved after her departure, the sad fact is that we are currently having to fight many of the battles of the 1980s all over again.
What always struck me about Thatcher was the gulf between rhetoric and reality. When she came into office, her arts minister, Norman St John-Stevas, endlessly repeated the Thatcherite mantra that there would be no "candle-end economies in the arts." Yet what actually happened? Her tenure began with a 4.8% cut to Arts Council grants and ended with one of 2.9%. In 1987 her arts minister, Richard Luce, announced that "the only test of our ability to succeed is whether we can attract enough customers." And, on one of the many occasions when she took Peter Hall to task for complaining, as director of the National Theatre, about arts underfunding, she pointed to the popularity of British theatre the world over. "Look," she said with menacing, jabbing finger, "at Andrew Lloyd Webber".
It is no accident that Thatcher seized on Lloyd Webber as a symbol of what theatre should be. He embodied everything of which she approved: entreprenuerial skill, a world-famous brand-name, the ability to make money. I enjoy a lot of Lloyd Webber's work but, as I argued in my book State of the Nation, it seemed apt that the musical should become the dominant form of the 1980s since it represented Thatcherism in action: what it celebrated was the triumph of individualism and profitability. Where British theatre in previous decades had been famed for its writers, actors and directors, in the 1980s it became identified with its musicals – Cats, Starlight Express, Les Miserables, The Phantom of the Opera, Miss Saigon. Even the big national companies were seduced into believing that a popular musical was a passport to survival.
Part of Thatcher's legacy is the lasting effect she had on our culture. But it's only fair to point out that there was a fightback, and that her values eventually came to be challenged by our more resilient dramatists. As early as 1980 Howard Brenton and Tony Howard wrote a satirical attack on Thatcherism, A Short Sharp Shock, which was produced at the Theatre Royal, Stratford East. It was broad, agitprop fun, but it says a lot about the times that St John-Stevas was forced to apologise in the Commons for its presentation in a subsidised theatre. The work was also prophetic in that, although Mrs Thatcher was its prime target, she was the most dynamic figure on stage. As in drama, so in life. She dominated every scene she was in.
Other dramatists were subtler and more circuitous in their attack on Thatcherite values. Caryl Churchill's still-potent Top Girls, first seen in 1982, showed its heroine running her own London employment agency; but part of Churchill's point was that society will never change as long as career-driven women feel obliged to behave like surrogate men (a point reinforced on TV's Spitting Image, where Thatcher was always portrayed as a balls-buster in a striped suit). In Serious Money (1987) Churchill also went on to nail the spirit of an age in which greed was good and virtually any amoral action was vindicated by profit.
As the 1980s progressed, more and more dramatists explored the psychology and consequences of Thatcherism. In The Secret Rapture (1988), David Hare suggested that the anger that fuelled a figure like Thatcher stemmed not just from fury at the vaccillating "wetness" of their colleagues but from some perceived deficiency within themselves. But, for me, the play that offered the sharpest attack on Thatcherite values came from the supposedly apolitical Alan Ayckbourn. In A Small Family Business (1987), without ever mentioning Mrs Thatcher but to devastatingly comic effect, Ayckbourn pinned down the essential contradiction in her beliefs: that you cannot simultaneously sanctify traditional family values and individual greed. If you do, implies Ayckbourn, you end up with a family that owes more to the Mafia than morality.
And Thatcher continues to fascinate British dramatists. In Little Madam (2007) James Graham explored the imaginative poverty of her Grantham upbringing, and she is also a peripheral presence in his play, This House, which focuses on parliamentary politics in the years immediately she came to power. In Peter Morgan's The Audience she is portrayed by Haydn Gwynne – who will, presumably, be going on stage tonight – as a woman in a tearing temper prepared to queen it over her monarch.
But, while I suspect her battering-ram persona and apparent lack of hinterland will long continue to haunt writers, her real legacy is to be found elsewhere: in the frightening fact that we are still having to argue that subsidy of the arts is a fruitful investment rather than a frivolous expenditure.
Stage books


Every year, nine in 10 of the nation's three million teachers participate in professional development designed to improve their content knowledge, transform their teaching, and help them respond to student needs. These activities, which can include workshops, study groups, mentoring, classroom observations, and numerous other formal and informal learning experiences, have mixed results in how they effect student achievement.
Research shows that professional learning can have a powerful effect on teacher skills and knowledge and on student learning. To be effective, however, it must be sustained, focused on important content, and embedded in the work of collaborative professional learning teams that support ongoing improvements in teachers' practice and student achievement.
A comprehensive new report released last week by researchers from Stanford University and the National Staff Development Council (NSDC) finds that while the United States is making progress in providing support and mentoring for new teachers and focusing on bolstering content knowledge, the type of support and on-the-job training most teachers receive is episodic, often fragmented, and disconnected from real problems of practice. The report also reviews promising strategies in high-performing nations and U.S. states.
The report – Professional Learning in the Learning Profession: A Status Report on Teacher Development in the U.S. and Abroad – documents some progress but many serious problems in teacher development today: Improvement in support for new teachers. According to the report, U.S. public schools have begun to recognize and respond to the need to provide more support for new teachers. Nationally, in 2003-04, more than two-thirds (68 percent) of public school teachers with fewer than five years of experience reported participating in a teacher induction program during the first year of teaching, and 71 percent reported being assigned some kind of mentor teacher.
Workshop overload. Research shows that professional development should not be approached in isolation as the traditional "flavor of the month" or one-shot workshop but go hand-in-hand with school improvement efforts. The report finds that teachers still take a heavy dose of workshops and do not receive effective learning opportunities in many areas in which they want help.
Little intensity, short duration. While rigorous studies indicate that intensive professional development efforts that offer an average of about 50 hours of support a year can make a significant impact on student achievement, raising test scores by an average of 21 percentage points, the majority of teachers in the United States (57 percent) receives no more than about two days (16 hours) of training in their subject areas. Fewer than one-quarter (23 percent) of all teachers receive more than 36 hours of professional learning in their subject areas.
Working in isolation. U.S. teachers report little professional collaboration in designing curriculum and sharing practices, and the collaboration that occurs tends to be weak and not focused on strengthening teaching and learning.
Major blind spots. Teachers are not getting adequate training in teaching special education or limited English proficient students. More than two-thirds of teachers nationally had not had even one day of training in supporting the learning of special education or LEP students during the previous three years, and only one-third agreed that they had been given the support they needed to teach students with special needs. Lack of utility. Teachers give relatively high marks to content-related learning opportunities, with 59 percent saying this training was useful or very useful. But fewer than half found the professional development they received in other areas, such as classroom management, to be of much value, despite the fact that they want more support in this area.
Out-of-pocket payments. U.S. teachers, unlike many of their colleagues around the world, bear much of the cost of their professional development. While most teachers were given some time off during the work day to pursue professional learning opportunities, fewer than half received reimbursement for travel, workshop fees, or college expenses.
Variation in support and opportunity among schools and states. A lower percentage of secondary school teachers reported participating in district-planned professional development than did elementary school teachers. Among states, Arkansas, Connecticut, New Hampshire, and Vermont had significantly higher proportions of teachers participating in professional learning than the national average.
Limited influence in decision-making. In many high-achieving nations where teacher collaboration is the norm, teachers have substantial influence on school-based decisions, especially in the development of curriculum and assessment, and in the design of their own professional learning. In the United States, however, less than one-fourth of teachers feel they have great influence over school decisions and policies in seven different areas noted in the SASS surveys. A scant majority feel that they have some influence over curriculum and setting performance standards for students, though fewer than half perceived that they had some influence over the content of their in-service professional development. And very few felt they had influence over school.
How is professional development at your school?


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ENGSO at the PyeongChang2018 Olympic and Paralympic Winter Games
A handful of ENGSO's representatives were involved in the Olympic and Paralympic Winter Games in February and earlier this month. Our Secretary General, Stefan Bergh, our Executive Committee member, Stavri Bello and our Communication Officer, Mariann Bardocz-Bencsik were all in PyeongChang and Gangneung, and now it's their turn to share their first-hand Olympic and Paralympic experience with you.
Stefan Bergh, Secretary General
"I was at the Olympic Games mainly in my capacity as Secretary General in the Swedish Sports Confederation. My federation works closely with the Swedish Olympic Committee and they have the operative responsibility for the Swedish participation in the Olympic Games.
The Games in PyeongChang were a great success. As far as I have seen the event has been well-organised. All the participants that I´ve met have been very satisfied.
I can also say that I´ve done some work for ENGSO. The Olympic Games was a good opportunity to meet representatives from different ENGSO member organisations, to network and to talk about upcoming ENGSO events."
Stefan Bergh in PyeongChang
Stavri Bello, Executive Committee member
"In my position as Secretary General of the Albanian National Olympic Committee, I have had the opportunity to attend the Olympic Games. These Games will be one of my special memories of the Olympics. The Olympic atmosphere was present from the arrival to Incheon Airport where groups of volunteers welcomed all participants and offered their help to better accommodate us with information on logistics and above all, made us feel the Olympic hospitality.
Everything was in place from the Opening Ceremony, throughout the events, and the enthusiasm of the spectators was fantastic.
Why were these Olympic Games so special? We all know the efforts of several parties led by the International Olympic Committee and the United Nations that aim to contribute to peace. It was fantastic to see the united Korean team at the Opening Ceremony. That was the most significant moment to understand the power of the Olympics and the power of sport. Regardless political differences, sport and Olympic spirit showed the world the power of unity, respect and that there are always opportunities of building a better world to live in peace."
The Albanian delegation: Erion Tola, athlete, Stavri Bello, Suela Mehilli, athlete and Kliton Muca, chief of mission
Mariann Bardocz-Bencsik, Communication Officer
"My experience at the Paralympic Games was beyond my expectations.


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Whilst the Digital TV revolution has taken over and called time on old analogue aerials, there is still a need for a powerful aerial on your roof or building if you want to guarantee the very best quality digital TV. Installing and fixing TV aerials is always best left to the experts, which is what we are here for at BNC Electrical Contractors.
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Download "United States Government 2005"
1. Which of these was the earliest document to contain principles of limited government that were later reflected in the United States Constitution?
1. Which of these was the earliest document to contain principles of limited government that were later reflected in the United States Constitution? Magna Carta. Petition of Right. English Bill of Rights.


text:
News Articles by Evelyn Adamson
Evelyn Adamson
In West Africa, clinic rescues starving babies
By Evelyn Adamson, posted September 25, 2015 in
WEST AFRICA (BP) -- Whipping desert winds fill the air with dust, which settles on the clinic's metal gate, muting its deep maroon color. A clinic worker opens the gate, and two grandparents step into the clinic with their 2-month-old grandson. Untying the wrap that holds the baby on her back, the grandmother slides him around in front and cradles him as she sits down. The baby's grandfather pulls up a chair and sits next to them. The emaciated baby lies motionless on his grandmother's lap. The simple move ...
By Evelyn Adamson, posted September 1, 2015 in Southern Baptist Compassion
A simple formula distribution project like this saves lives in sub-Saharan Africa.
Syrian refugees to hit 4M; Baptists continue serving
By Evelyn Adamson, posted April 17, 2015 in Baptist Global Response, Immigration
LONDON (BP) -- Syria entered its fifth year of conflict in March with the grim report that an estimated 220,000 people have been killed since fighting began in early 2011. In addition, registered refugee numbers soon will hit the 4 million mark, according to the Office of the United Nations High Commissioner for Refugees (UNHCR).
Flood victims in Southern Africa receive aid
By Evelyn Adamson, posted February 2, 2015 in International Mission Board, SBC News
JOHANNESBURG (BP) -- Severe rains have hammered Madagascar, Mozambique and Malawi in recent weeks, displacing more than 200,000 people and leaving hundreds more missing or dead. Baptist Global Response and International Mission Board personnel rushed aid to vital areas, delivering food and supplies to families with critical needs across southern Africa. Rivers swelled beyond capacity, converted plains into lakes, and completely erased villages. In Malawi, a reported 275 people are missing or assumed dead. Mozambique reported there were 11,000 homes destroyed and 88 fatalities.
FIRST-PERSON: Ebola on both sides
By Evelyn Adamson, posted October 3, 2014 in International Mission Board, SBC News
As Ebola continues to make headlines, IMB writer Evelyn Adamson examines the personal impact Ebola has left on communities across West Africa and in the United States.
Gospel shared with Ukrainians in Sochi
By Evelyn Adamson, posted March 10, 2014 in
SOCHI, Russia (BP) -- After a long day of performing with her drama team at the recent Winter Olympics in Sochi, Tamara Wasylyshyn wanted nothing more than to step into the American fast food chain down the street, eat dinner and rest.
Bible translation is their shared ministry
By Evelyn Adamson, posted February 24, 2014 in
SOUTHEAST ASIA (BP) -- The constant tick, tick, tick of computer keys provides the backdrop as Don Patrick* and Rith Jaya* compare notes on flickering laptop screens. The men also swish the pages of a dictionary as they work together.
Baptist troubadours strum Gospel in Sochi
SOCHI, Russia (BP) -- Members of the Earl Brackin Band sing and strum their traditional bluegrass instruments, rendering a soul-stirring version of "I'll Fly Away," as dozens of Olympics fans gather to listen, some of whom capture the music on their smartphones.
Earl Brackin, minister of worship at Church on the Hill in Dalton, Ga., said prior to leaving for Russia, "In Sochi, we'll be like troubadours. Since bluegrass bands don't need electricity, we can set up and play anywhere -- street corner, open market, hotel, café, anywhere there is space for us to stand."
Winter Olympics: Baptists trek to Sochi to share their faith
By Evelyn Adamson, posted February 7, 2014 in
SOCHI, Russia (BP) -- Amid tight security, the 2014 Winter Olympics commenced with impressive opening ceremonies, while Baptist volunteers from across the United States arrived to be part of the international festivities. Inside Sochi's "ring of steel," consisting of 40,000 armed Russian troops, anti-aircraft weapons and a myriad of military surveillance tactics, the five Olympic rings welcomed thousands of athletes, fans, diplomats and dignitaries to the Sochi Games. [QUOTE@right@180="Who knows what God is up to here? It's humbling to have a front row seat."
-- Southern Baptist volunteer in Sochi]President Vladimir Putin ushered in the Games during the opening ceremonies at Fisht Olympic Stadium -- stirring a sense of competition, camaraderie and inspiration. Among those present is a select group partnering under the name Engage Sochi. Their purpose is simple: to make a difference for Christ before, during and after the 2014 Winter Olympics. The Southern Baptist volunteers journeyed thousands of miles despite persistent media attention to fears of terrorist threats. Engage Sochi is a network of Southern Baptists seeking to create opportunities for meaningful conversations with those living and working in Sochi or who are attending the Games. Volunteers hail from across the United States, including Oklahoma, Missouri, Colorado, Georgia and Alabama. Scheduled to perform are the Singing Men of Oklahoma, Woman's Missionary Union drama teams and ministry teams from Missouri and Colorado intent on sharing the love of Christ. Volunteers engage people throughout the community, walking in the knowledge that thousands around the world are praying for them and for Sochi during the coming weeks. "Never in our lives have we felt the prayers of people so tangibly," one volunteer said. "Even tonight, a casual conversation on the train turned into a person helping us, and a really good local contact was made." As people respond and ask questions, steps are taken to ensure that once they return home, they are connected with a local community of believers, regardless of where they live throughout the world. To stay connected with Engage Sochi during the 2014 Winter Olympic Games, visit the Facebook page for the outreach, Facebook.com/EngageSochi and use its hashtag for the games -- #pray4sochi. Engage Sochi prayer request The North Caucasus region of Russia, in which Sochi sits, has long suffered from political unrest. ...
Sewing dresses garners income & moments to share her faith
SOUTHEAST ASIA (BP) -- Uncertainty rocked Vanna Keo* after her husband Kith* accepted Christ. She had never met any Christians before, and now her husband was one. In supporting her husband, Keo agreed to meet Don and Dayla Patrick*, IMB workers in Southeast Asia for more 15 years. The Patricks were the ones who shared the Gospel with her husband and led him to Christ.


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New 2011 Honda Accord is very beautiful sport car and very big too but still very fuel efficient for that size. It is even comparable to sports pedigree models while it follows the blueprint of family four-door vehicles. Honda is also looking to incorporate a smoother skin for this vehicle model to deliver the same swept-back look of the coupe model.


text:
Baiersbronn es un municipio alemán perteneciente al distrito de Freudenstadt en el estado federado de Baden-Wurtemberg. Le pertenecen los barrios de Friedrichstal, Mitteltal, Obertal, Tonbach, Klosterreichenbach, Röt- Schönegründ, Huzenbach, Schwarzenberg, Schönmünzach y Schönmünz. En total, el municipio tiene unos 16 000 habitantes.

Puntos de interés
 Lago Buhlbach
 Parque Cultural Vidriería Buhlbach (Kulturpark Glashütte Buhlbach)
 Ruina del castillo de Tannenfels
 Museo de Cuentos de Hauff

Referencias

Enlaces externos

  (en alemán) Sitio web de Baiersbronn
 Sitio web del Parque Cultural Vidriería Buhlbach

Localidades de Baden-Wurtemberg


text:
Detroit Lions Opinion
Top 10 Lions plays of 2013: Nos. 6 and 5
The countdown of the Detroit Lions' top plays of 2013 continues with two very different and very impressive plays.
By Jeremy Reisman@DetroitOnLion Jan 28, 2014, 4:01pm EST
Share All sharing options for: Top 10 Lions plays of 2013: Nos. 6 and 5
Mike DiNovo-USA TODAY Sports
Our next two plays on the countdown are polar opposites. One was a play that clearly was going to decide the game. The other, a seemingly unimportant play in the middle of the third quarter. One was a display of how the play of one person can change an entire game; the other, an example of how teamwork can produce explosive results. And the stars of each play, Nick Fairley and Reggie Bush, well, let's just say they have different body types.
6. Nick Fairley blows up Matt Forte in the backfield FTW
The season was slowly slipping away (you know, before it actually did). The Detroit Lions were in prime position to complete the season sweep of the Chicago Bears and take a huge lead in the NFC North. But that all seemed to be fading away into a Kool-Aid fueled pipe dream when Josh McCown easily drove the Bears to a last-minute touchdown. But Chicago was still a 2-point conversion away from sending the game into overtime (which I am still convinced they would have won on some devastating, fluky play). But we would never see such an overtime.
WATCH THE PLAY HERE
The play call from the Bears was a bit curious. Forte was averaging less than 2 yards a carry on the day, and he hadn't had a rush of over 7 yards all game. But the Bears didn't need 7 yards, they needed just 1. So they went shotgun, spread out their receivers and tried to run up the gut. Bad idea.
Before Forte even gets the ball, Fairley has split two linemen and has free rein into the backfield. Fairley doesn't even have to fully wrap up Forte to take him down. What's really interesting about this play is that the Lions may not have even needed Fairley's help on it.
DeAndre Levy had shed his block and was heading to the backfield. Meanwhile, Willie Young had sealed off the edge, while Ndamukong Suh blocked any hope of a cutback lane. Forte had no chance.
The Lions won the game because of this play and took a commanding lead in the NFC North. And they all lived happily ever after.
5. In his Lions debut, Reggie Bush takes a screen 77 yards for six
The Lions made national headlines with their offseason acquisition of Bush. Hopes were that Bush would add the explosive element to Detroit's offense that had been missing since Jahvid Best was forced into retirement by concussions. It didn't take long for Bush to convince the Lions they had made the right choice.
This was just a perfectly executed screen.
Immediately Rob Sims, Dominic Raiola and Larry Warford get downfield (but not too far downfield to draw a penalty). As Matthew Stafford lays a nice pass to the cutting Bush, Reggie has a cavalcade of blockers in front of him.
But Reggie doesn't even need those blockers. He turns on the turbo jets and runs past everybody. Bush is running so fast, you can easily imagine that blurred No. 25 on the back of his jersey is really a No. 44 and suddenly I'm back in 2011 and everything with the world is good again.
Of course, my favorite part of this play is not the blocking or even the fact that Bush scored a touchdown. No, my favorite part of this play is the impromptu race that broke out between Bush and Patrick Edwards.
With over 50 yards left, Bush had a 4-yard lead:
But Edwards quickly closes in on Bush, and it's a photo finish:
Bush leaps at the last second and beats Edwards by the nose of the football. Sadly, shortly after the race, Edwards was put down and never heard of again. Tough break, kiddo.
Our third honorable mention comes from DeAndre Levy, who broke into the countdown earlier. This play was not nearly as physically impressive as our No. 9 play, but it was Levy's first trip into the end zone since 2010.
Levy's pick-six was a huge play in a close game. But I couldn't in good faith sneak it into the top 10, because this was just a terrible decision by Carson Palmer.
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2013 POD Awards: Game of the Year
Lions notes: From 0-16 to the Super Bowl
2014 NFL mock draft: Two-round mock for Lions
Tuesday Lions open thread
Scott Linehan to be hired by Cowboys, according to report
Wrapping up the Lions' 2013 season
Closing the book on the Lions' 2013 season


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