text:
\section{Introduction}
\subsection{Magnetism and rotation in the main sequence A and B stars}

Between about 1.5 and 10 M$_{\odot}$, at spectral types A and B, about 5\% of main sequence (MS) stars have magnetic fields with characteristic strengths of about 1 kG. Such stars also show important chemical peculiarities and are thus usually called the magnetic chemically peculiar Ap/Bp stars. Two hypotheses have been proposed to explain the origin of their magnetic fields: the core dynamo hypothesis and the fossil field hypothesis. The core dynamo hypothesis assumes that a magnetic field is generated in the convective core of the main sequence (MS) Ap/Bp stars, and then diffuses towards the surface. On the contrary, the fossil field hypothesis assumes that the stellar magnetic fields are relics from the field present in the parental interstellar cloud or possibly generated early in their evolution, by a dynamo that has ceased to operate. It implies that magnetic fields can (at least partially) survive the violent phenomena accompanying the birth of stars, and can also remain throughout their evolution and until at least the end of the MS, without significant regeneration.

According to the fossil field model, some pre-main sequence (PMS) stars of intermediate mass should be magnetic. Many such PMS stars are identifiable observationally as Herbig Ae/Be (HAeBe) stars. However no magnetic field was observed up to recently in these stars (except in HD~104237, Donati et al., 1997). {\it Can we obtain observational evidence of the presence of magnetic fields
in PMS A/B stars, as predicted by the fossil field hypothesis? If some HAeBe stars are discovered to have magnetic fields, is the fraction of magnetic to non-magnetic HAeBe stars the same as the fraction for main sequence stars? Are the magnetic fields in HAeBe stars strong enough and of appropriate geometry to explain those of the Ap/Bp stars?}

Chemical peculiarities and magnetism are not the only characteristic properties observed in the Ap/Bp stars. Most magnetic MS stars have rotation periods (typically of a few days) that are several times longer than the rotation periods of non-magnetic MS stars (a few hours to one day). It is usually believed that magnetic braking, in particular during PMS evolution when the star can exchange angular momentum with its massive accretion disk, is responsible for this slow rotation (St{\c e}pie{\'n}, 2000). An alternative to this picture involves a rapid dissipation of the magnetic field during the early stages of PMS evolution for the fastest rotators, due to strong turbulence induced by rotational shear developed under the stellar surface, as occurs in solar-type stars (e.g. Ligni\`eres, 1996). In this scenario, only slow rotators could retain their initial magnetic fields, and evolve as magnetic stars to the main sequence. So another question to be addressed is the following: {\it does the magnetic field control the rotation of the star, or does the rotation of the star control the magnetic field?}

To answer to these questions we adopt two strategies. The first consists of observing the brightest "field" HAeBe stars in order to detect magnetic fields, to measure rotation velocities and finally to make a statistical study to be compared to the statistical properties of magnetism and rotation of the main sequence A/B stars. The second strategy consists of observing HAeBe stars in young open clusters and associations. Observing stars in a single cluster or association will provide us with stars of approximately the same age and initial conditions (chemical composition, angular momentum, environment). Then, by selecting members of open clusters and associations of various ages, we hope to be able to disentangle "evolutionary" effects from "initial conditions" effects. Thanks to both studies we will therefore improve our understanding  of the evolution of the magnetic field during the pre-main sequence phase, and its impact on the evolution of the stars.

\subsection{Evolution of intermediate-mass stars}

The MS A and B stars are intermediate-mass (1.5 to 15~M$_{\odot}$) stars. The main difference between MS intermediate mass stars and MS low-mass star is their internal structure. A low-mass star has a radiative core and a convective envelope, while A and B stars have a convective core and a radiative envelope. In low-mass stars, magnetic fields are generated by dynamos in their convective envelope. We understand therefore the necessity to involve a different origin for the magnetic field of the intermediate mass stars.

During their pre-main sequence phase the intermediate and low mass stars follow a different evolution, which is fundamental in understanding the origin of magnetic fields. In Fig. \ref{fig:hr} (left) are plotted the PMS evolutionary tracks (full black lines) computed with the CESAM code (Morel 1997), for different masses (from 1.5 to 20 M$_{\odot}$). The PMS evolution starts with a fully convective phase on the Hayashi track (the vertical part). During many years, the fossil field hypothesis was considered to be unlikely because magnetic field relics would have been dissipated during this convective phase. However Palla \& Stahler (1993) modelled proto-stellar evolution until the star becomes optically visible by clearing away its opaque envelope. They defined the birthline as the locus in the HR diagram of these newly formed stars, and they computed it using two different mass accretion rates during the protostellar phase : 10$^{-5}$~M$_{\odot}$.yr$^{-1}$ and 10$^{-4}$~M$_{\odot}$.yr$^{-1}$ . Both birthlines are plotted in Fig. \ref{fig:hr} (left) in small dashed-lines. The zero-age main-sequence (ZAMS) computed with CESAM is also plotted in long dashed-line. The PMS lifetime of a star is therefore from the birthline to the ZAMS. It implies that the Hayashi phase of intermediate mass stars is considerably reduced for stars between 1.5 $M_{\odot}$ and 3 $M_{\odot}$ and disappears totally above 3~$M_{\odot}$. Fossil magnetic fields can therefore survive during the PMS evolution of intermediate mass stars.

In Fig. \ref{fig:hr} are also plotted the convective envelope disappearance and the convective core appearance lines, calculated with CESAM. During the PMS phase stars experience three different internal structures: either a radiative core and a convective envelope, or a totally radiative interior, or a convective core and a radiative envelope. The PMS stars of intermediate mass stars are therefore very suitable laboratories to test both hypotheses of magnetic field origin.

\begin{figure}[t!]
\centering
\includegraphics[width=6cm]{alecian_fig1.ps}
\hfill
\includegraphics[width=6cm]{alecian_fig2.ps}
\caption{{\it Left: }  PMS evolutionary tracks (full black line), convective envelope disappearance (red dot-dashed line) and convective core appearance (red dot-dot-dot-dashed line), calculated with CESAM (Morel 1997). The black long-dashed line is the ZAMS and the blue small-dashed lines are the birthlines for 10$^{-5}$ and 10$^{-4}$ $M_{\odot}$.yr$^{-1}$ mass accretion rates (Palla \& Stahler 1993). {\it Right: } Field (circles) and cluster (triangles) HAeBe stars. The large cross in the upper-right of the panel is the mean error bars in luminosity and temperature of the undetected stars.}
\label{fig:hr}
\end{figure}

\subsection{The Herbig Ae/Be stars}

The Herbig Ae/Be stars are intermediate mass stars displaying emission lines in their spectrum. They are distinguished from the classical Be stars by their abnormal extinction law and association with nebulae. Most of them are still in the pre-main sequence phase, and therefore the evolutionary progenitors of the MS A and B stars.

HAeBe stars display many observational phenomena often associated with magnetic activity. First, highly ionised lines are observed in the spectra of some stars (e.g. Bouret et. al., 1997), and X-ray emission has been detected coming from the environments of HAeBe stars (e.g. Hamaguchi et al., 2005). In active cool stars, many of these phenomena are produced in hot chromospheres or coronae. Some authors have also mentioned rotational modulation of resonance lines which they speculate may be due to rotation modulation of winds structured by magnetic field (e.g. Catala et al. 1989).

In the literature we find many clues to the presence of circumstellar disks around these stars, from spectroscopic and photometric data (e.g. Vink et al. 2002). Recently, using coronographic and interferometric data, some authors have also found direct evidence of circumstellar disks around these stars (e.g. Eisner et al. 2003). These disks show similar properties to the disks of their low mass counterparts (Natta et al. 2001), the T Tauri stars, whose emission lines have been explained by magnetospheric accretion models (Muzerolle et al. 2001). Finally Muzerolle et al. (2004) have sucessfully applied their magnetospheric accretion model to one HAeBe star to explain the emission lines in its spectrum.

For all these reasons we suspect that the HAeBe stars may host large-scale magnetic fields that should be detectable with current instrumentation. However, many authors have tried to detect such fields without much success (Catala et al. 1989, 1993; Donati et al. 1997; Hubrig et al. 2004; Wade et al. 2007). The previous instruments were limited either by their spectral range, or by their spectral resolution, or by low efficiency. However, in 2005 a new high-resolution spectropolarimeter, ESPaDOnS, was installed at the Canada-France-Hawaii telescope. This powerful new instrument has provided us with the capability to sensitively survey many HAeBe stars in order to investigate rotation and magnetism in the pre-main sequence stars of intermediate mass.

\section{Observations}

Our data were obtained using the high resolution spectropolarimeter ESPaDOnS installed on the 3.6 m Canada-France-Hawaii Telescope (CFHT, Donati et al., in preparation; Neiner 2008, these proceedings) during several scientific runs.

We used this instrument in polarimetric mode, measuring Stokes $I$ and $V$ spectra of 65000 resolution. The data were reduced using the "Libre ESpRIT" package especially developed for ESPaDOnS, and installed at the CFHT (Donati et al. 1997; Donati et al. in preparation).

We then applied the Least Squares Deconvolution procedure to all spectra (Donati et al. 1997), in order to increase our signal to noise ratio. This method assumes that all selected lines of the intensity spectrum have a profile of similar shape. Hence, this supposes that all lines are broadened in the same way. We can therefore consider that the observed spectrum is a convolution between a profile (which is the same for all lines) and a mask including all choosen lines of the spectrum. We therefore apply a deconvolution to the observed spectrum using the mask, in order to obtain the average photospheric profiles of Stokes $I$ and $V$. In this procedure, each line is weighted by its signal to noise ratio, its depth in the unbroadened model and its Land\'e factor. For each star we used a mask computed using "extract stellar" line lists obtained from the Vienna Atomic Line Database (VALD)\footnote{http://www.astro.univie.ac.at/$\sim$vald/}, with effective temperatures and $\log g$ suitable for each star (Wade et al. in prep.). We excluded from this mask hydrogen Balmer lines, strong resonance lines, lines whose Land\'e factor is unknown and emission lines. The results of this procedure are the mean Stokes $I$ and Stokes $V$ LSD profiles.

\section{Field Herbig Ae/Be stars study}
\subsection{Our sample}

Our sample contains 55 stars which have masses ranging from 1.5 M$_{\odot}$ to 20 M$_{\odot}$, selected in the catalogues of Th\'e et al. (1994) and Vieira et al. (1993) with a visual magnitude brighter than 12. In Fig. \ref{fig:hr} (right, circle) are plotted the stars of our sample in an HR diagram. We observe a variety of internal structure of stars in our sample will allow us to test both the fossil field hypothesis and the core dynamo hypothesis.

\subsection{The magnetic field}

\begin{figure}[t]
\centering
\includegraphics[width=6.cm, angle=90]{alecian_fig3.ps}
\caption{Stokes $I$ (bottom) and Stokes $V$ (top) LSD profiles of the 4 magnetic stars observed with ESPaDOnS (left), of 2 undetected stars (middle) and of the 2 magnetic stars observed with SemelPol (right). Note the amplification factor in $V$.}
\label{fig:compil}
\end{figure}

The combination of ESPaDOnS and the LSD method has allowed us to discover four new magnetic HAeBe stars. The Zeeman signatures in the Stokes $V$ profiles of the four magnetic HAeBe stars are plotted in Fig. \ref{fig:compil} on the left. These can be compared to some undetected stars (stars in which we have not detected magnetic fields) in the middle. We observe that these signatures are located at the same position as the absorption line, and are as broad as the intensity profile. They are therefore characteristic of the presence of magnetic fields in the stars. As our sample contains 55 stars, the first conclusion that we draw is that ~7\% of our sample HAeBe stars are magnetic.

In order to characterise these magnetic fields, we monitored the four detected stars during many nights. We recorded variations of the Zeeman signature with time for all stars, except one (HD~190073), which exhibits a constant profile. To model these variations we assume the oblique rotator model described in Landstreet (1970). This model assumes a dipole of intensity $B_{\rm d}$ placed at a distance $d_{\rm dip}$ of the center of the star, on the magnetic axis inside the star, and inclined with an angle $\beta$ to the rotation axis. The rotation axis make an angle $i$ with the line of sight. As the star rotates with a period $P$, the magnetic configuration at the visible surface of the star, and therefore the Stokes $V$ profile, changes with the rotation phase. We calculated on each point of the observable surface of the star a local intensity $I(\theta,\phi)$ profile using a Gaussian of instrumental width placed at the local velocity. Using the weak field approximation (Landi degl'Innocenti \& Landi degl'Innocenti 1973), we calculated the local Stokes $V(\theta,\phi)$ profile as a function of ${\rm d}I(\theta,\phi)/{\rm dv}$ and the local magnetic field projected on the line of sight $b_{\ell}(\theta,\phi)$. We then integrated $I(\theta,\phi)$ and $V(\theta,\phi)$ over the stellar surface, using the linear limb-darkening law with a suitable coefficient value for the star (Claret 2000), in order to get the Stokes $I$ and $V$ profiles. This model is therefore dependent on 6 parameters: the rotation period $P$, the reference time of the rotation phase $T_0$, the magnetic obliquity $\beta$, the inclination of the rotation axis $i$, the dipole intensity $B_{\rm d}$, and the position $d_{\rm dip}$ of the dipole on the magnetic axis with respect to the center of the star.

We fitted the observed Stokes $I$ profiles to the synthetic ones, described above, then we calculated a grid of synthetic Stokes $V$ profiles by varying the 6 parameters. Finally, we fitted all observed $V$ profiles of a single star by a $\chi^2$ minimisation. The best model of HD~200775 is superimposed on the observed profiles in Fig. \ref{fig:fitv}, while the best model parameters are summarised in Table \ref{tab:fitv} for all the stars. In the case of V380 Ori we found two possible models. We do not have yet enough data to choose between them. In all cases the oblique rotator model is sufficient to reproduce our observations.

\begin{figure}[t]
\centering
\includegraphics[width=6.cm, angle=90]{alecian_fig4.ps}
\caption{Stokes $V$ profiles of HD~200775 superimposed on the synthetic ones, corresponding to our best fit. The rotation phase and the error bars are indicated on the left and on the right of each profile, respectively (Alecian et al. 2008a).}
\label{fig:fitv}
\end{figure}

\begin{table}[t]
\caption{Fundamental, geometrical and magnetic parameters of the magnetic Herbig Ae/Be stars. References : 1 : Alecian et al. (2008a), 2 : Folsom et al. (2008), 3 : Alecian et al., in prep., 4 : Catala et al. (2007).}
\label{tab:fitv}
\centering
\begin{minipage}[t]{16cm}
\begin{tabular}{lcccccccc}
\hline
\footnotesize{Star}   & \footnotesize{S.T}. & \footnotesize{P}    & \footnotesize{$B_{\rm P}$} & \footnotesize{$\beta$ ($^{\circ}$)} & \footnotesize{$i$ ($^{\circ}$)} & \footnotesize{$d_{\rm dip}$} & \footnotesize{$B_{\rm P (ZAMS)}$} & \footnotesize{Ref.} \\
         &         & \footnotesize{(d)}  & \footnotesize{(kG)}             &                                 &                         & \footnotesize{$R_*$}             & \footnotesize{(kG)}                          &        \\
\hline
\footnotesize{HD 200775} & \footnotesize{B2}  & \footnotesize{4.3281}         & \footnotesize{1.0}             & \footnotesize{55}            & \footnotesize{60}            & \footnotesize{0.05} & \footnotesize{3.6}                                             & 1 \\
\footnotesize{HD 72106}   & \footnotesize{A0}  & \footnotesize{0.63995}     & \footnotesize{1.3}          & \footnotesize{60}            & \footnotesize{23}            & \footnotesize{0}    & \footnotesize{1.3}                                             & \footnotesize{2} \\
\footnotesize{V380 ori}
& \footnotesize{A2}  & \footnotesize{$[7.6,9.8]$} & \footnotesize{1.4}          & \footnotesize{$[90,85]$} & \footnotesize{$[36,49]$} & \footnotesize{0}    & \footnotesize{2.4} & \footnotesize{3} \\
\footnotesize{HD 190073
& \footnotesize{A2}  &                   & \footnotesize{$[0.1,1]$} & \footnotesize{$[0,90]$}   & \footnotesize{$[0,90]$}   &       & \footnotesize{$[0.4,4]$}                                    & \footnotesize{4} \\
\hline
\end{tabular}
\end{minipage}
\end{table}

This method is very efficient if we observe variations in the Stokes $V$ profiles. However in the case of HD~190073, no such variations are observed. To explain this we propose 3 hypotheses:  either the star is seen pole-on, or the magnetic obliquity is null and the magnetic field is axisymetric, or the rotation period of the star is very long. All these hypotheses are consistent with a dipolar field inside the star, which is further strengthened by the fact that the Zeeman signature is a simple bipolar signature which is stable over more than 2 years.

Finally, we mention two other detections obtained using the SemelPol polarimeter and the UCLES spectrograph at the Anglo-Australian Telescope (AAT) (Semel et al. 1993, Donati et al. 1997). The first is HD~104237, which was discovered to be magnetic by Donati et al. (1997), and which has been recently confirmed (Wade et al., in preparation). The second is HD 101412, discovered to be magnetic by Wade et al. (2007) using FORS1 at VLT, and which has been recently confirmed using SemelPol. The Zeeman signatures are plotted in Fig. \ref{fig:compil} on the right, and are typical signatures of a magnetic field inside the star. We still don't have enough data to characterise their magnetic fields, but the simple signatures are consistent with organised fields.

\subsection{The rotation}

In order to study the rotation during the PMS and MS phases, as well as the magnetic braking hypothesis, we measured the projected rotational velocities ($v\sin i$), by performing a Least-Squares fit to the LSD $I$ profiles of each star of our sample. The fitted function is the convolution of a rotation function (for which $v\sin i$ is a free parameter in the fit) and a gaussian whose width is fixed and computed from the spectral resolution and the inferred macroturbulent velocity (Gray 1992). The free parameters of the fitting procedure are the centroids, depths, and $v\sin i$.

In our study, we separated the stars of our sample in two different groups: the magnetic HAeBe stars, and the normal HAeBe stars which contains the non-magnetic and non-multiple stars (as the tidal interactions between both components of a binary system are braking both stars, we prefer to not include them in our study of the rotational evolution during the PMS phase).

In Fig. \ref{fig:rot1} are plotted the distributions of the $v\sin i$ of the magnetic HAeBe stars (left) and the normal HAeBe stars (right). Note that the binsize and the velocity scale are different in each case. We observe that the $v\sin i$ of the magnetic HAeBe stars are significantly lower than the $v\sin i$ of the normal ones: 4 magnetic HAeBe stars have a $v\sin i$ lower than 15~km.s$^{-1}$, while none of the normal HAeBe stars have a $v\sin i$ lower than 20~km.s$^{-1}$. Even though the inclination angles are not known and the true equatorial velocities of the stars are not known, it is clear that the magnetic HAeBe stars, as a population, are slower rotators than the normal HAeBe stars. We therefore conclude that the magnetic HAeBe stars seem to have been more braked than the normal ones.

\begin{figure}[t!]
\centering
\includegraphics[width=4cm]{alecian_fig5.ps}
\includegraphics[width=4cm]{alecian_fig6.ps}
\caption{$v\sin i$ histogram in number of stars, of the magnetic HAeBe stars ({\it left}) and of the normal HAeBe stars ({\it right}).}
\label{fig:rot1}
\end{figure}

PMS stars are still contracting towards the MS, therefore their radius is diminishing with time and their rotational velocity should increase towards the MS (assuming angular momentum conservation). In order to compare the rotation velocities of our normal HAeBe stars sample to those of the normal MS A/B stars, we compared the position in the HR diagram of each HAeBe star with CESAM evolutionary tracks. We inferred the mass, the actual radius and the age of the stars of our sample. We also inferred the radius that each star will have on the ZAMS, in order to compute their $v\sin i$ on the ZAMS. As the rotational velocity is slightly varying during the MS phase compared to the PMS phase, our distribution of $v\sin i$~(ZAMS) can be directly compared to the distribution of the $v\sin i$ of normal A/B stars. In Fig. \ref{fig:rot2} are plotted the distribution of the observed $v\sin i$ of normal HAeBe stars (left), their computed $v\sin i$ on the ZAMS (middle), and the observed $v\sin i$ of the normal A/B stars (right) from the catalogue of Royer et al. (2007). A Maxwellian function has been fitted to each distribution and is superimposed in full lines in Fig. \ref{fig:rot1}.

First we observe small but important differences between the actual $v\sin i$ and the ZAMS $v\sin i$ of HAeBe stars. The mode and the root mean square (rms) velocities of the Maxwellian function are respectively 91 km.s$^{-1}$ and 112 km.s$^{-1}$ for the actual $v\sin i$, and 136 km.s$^{-1}$ and 167 km.s$^{-1}$ for the ZAMS $v\sin i$. This slower and narrower $v\sin i$ distribution reflects the large range of ages and radii of the HAeBe sample. However these effects are small compared to what is expected during the entire PMS phase, according to the angular momentum conservation ($v\sin i$ should increase by a factor between 2 and 3, rather than 1.5 as observed). We explain this by the fact that most of our sample have less than 50\% of their PMS evolution remaining, during which the radius decrease is very small compared to the first part of the PMS phase (Alecian et al., in prep.). Our sample misses stars accomplishing the first half of their PMS phase, during which we cannot therefore conclude anything about the rotational evolution.

Secondly we observe a strong similarity between the predicted ZAMS $v\sin i$ of the HAeBe stars and those of the normal A/B stars: the modes and the rms velocities of the fitted maxwellian functions are respectively 136 km.s$^{-1}$ and 167 km.s$^{-1}$ for the ZAMS $v\sin i$ of the HAeBe sample, and 126 km.s$^{-1}$ and 154 km.s$^{-1}$ for the normal A/B stars. This suggests that the evolution of the PMS star from their actual age to the ZAMS is consistent with angular momentum conservation evolution.

\begin{figure}[t!]
\centering
\includegraphics[width=4cm]{alecian_fig7.ps}
\hfill
\includegraphics[width=4cm]{alecian_fig8.ps}
\hfill
\includegraphics[width=4cm]{alecian_fig9.ps}
\caption{$v\sin i$ histogram in percentage of stars of the normal HAeBe stars ({\it left}), of the normal HAeBe stars evolved to the ZAMS ({\it middle}) and of the normal A/B stars ({\it right}).}
\label{fig:rot2}
\end{figure}

\section{Herbig stars in young open clusters}

Motivated by these results we decided to go further and to observe HAeBe stars in young open clusters and associations. We selected Herbig members of three clusters: NGC 2244, NGC 2264 and NGC 6611, from the catalogues of Park \& Sung (2002), Park et al. (2000) and de Winter et al. (1997).

We observed 17 stars in NGC 2244, 27 stars in NGC 2264 and 17 stars in NGC 6611, which are plotted on the HR diagram in Fig. 1 (left, triangles). We detected magnetic fields in one star of each cluster: W601 (NGC~6611), OI~201 (NGC 2244) and NGC~2264~83 (Fig. \ref{fig:autre}).

The detection of W601 is very interesting, as this is our only detection of magnetic field in a fast rotator (${\rm v}\sin i\sim180$~km.s$^{-1}$). Furthermore, this star is very young ($<1\;$Myr) compared to OI~201 ($\sim2\;$Myr) and NGC~2264~83 ($\sim6\;$Myr). The two former have similar spectral type: B1.5 and B1 respectively, but W601 rotates with  ${\rm v}\sin i\sim180$~km.s$^{-1}$, while OI~201 rotates with only ${\rm v}\sin i\sim25$~km.s$^{-1}$ (Alecian et al. 2008b). These stars may provide us with clues about angular momentum evolution during the pre-main sequence phase.

\begin{figure}[t]
\centering
\includegraphics[width=4cm, angle=90]{alecian_fig10.ps}
\caption{Stokes $I$ (bottom) and Stokes $V$ (up) LSD profiles plotted for W601, OI~201 and NGC 2264 83 (Alecian et al. 2008b).}
\label{fig:autre}
\end{figure}

\section{Conclusion}

Our spectropolarimetric study of Herbig Ae/Be stars among field and cluster stars has brought new strong arguments in favour of the fossil field hypothesis to explain the origin of the magnetic fields of the intermediate mass stars:
\begin{enumerate}
\item The projection of the magnetic field incidence of A/B stars onto the PMS phase predicts between 2 and 10 \% of magnetic PMS stars (Power et al., in prep.). This is consistent with our results: from our investigation, we fins that 7\% of HAeBe stars are magnetic.
\item The magnetic HAeBe stars host large-scale organised magnetic fields, similar to the Ap/Bp stars.
\item Using the actual radius and the predicted ZAMS radius of the field magnetic HAeBe stars and assuming magnetic flux conservation, we predict that their magnetic field intensities on the ZAMS will be between 0.4 and 4 kG (Table \ref{tab:fitv}). This is of the same order of magnitude as the magnetic intensities of the Ap/Bp stars.
\end{enumerate}
 Furthermore, in order to confront the fossil field hypothesis and the core dynamo hypothesis, we plotted in the HR diagram of Fig. \ref{fig:hr} (right panel) all the magnetic HAeBe stars, as well as the undetected field and cluster stars. We observe that 5 stars among the 8 magnetic HAeBe stars are in the {\bf totally radiative zone}. Although the error bars are large, one of these is confidently in the totally radiative zone, including its error bars on temperature and luminosity. On the other hand, all 8 magnetic HAeBe stars host the same type of magnetic fields: a large-scale organised magnetic field. We therefore conclude that presence of core convection does not appear to be responsible for the presence of magnetic fields in HAeBe stars. The magnetic fields of the intermediate mass stars are therefore {\bf very likely of fossil} origin.

The study of the rotation of field HAeBe stars leads to the conclusion that the magnetic HAeBe stars are more braked than the normal (non-magnetic and non-binary) ones. We also show that the evolution of the PMS stars from the HAeBe ages to the ZAMS is {\bf consistent with angular momentum conservation}. On the other hand our field HAeBe sample is too old to study the angular momentum evolution during the early stages of the PMS phase: most of our sample has already completed at least 40\% of their PMS track. Our HAeBe cluster sample contains very young PMS stars and will allow us to better understand stellar angular momentum evolution at all stages of the PMS phase.


The Bihar State Power (Holding) Company Ltd., Patna has released the final result for the Assistant Operator, Junior Line Man, Switch Board Operator - II, Technician Gr.-IV examination held against the Employment Notice No. - 8/2018.
NEW DELHI: The Bihar State Power (Holding) Company Ltd., Patna has released the final result for the Assistant Operator, Junior Line Man, Switch Board Operator - II, Technician Gr.-IV examination held against the Employment Notice No. - 8/2018.
The candidates, who have appeared for the examination conducted on November 3 and 4, 2018, can check their result from the official BSPHCL website - http://bsphcl.bih.nic.in.
The result has been published in the PDF format, and the posts have been allotted to the selected candidates against ENN-8/2018.
The BSPHCL has also mentioned the requirement of the documents, if any, against the name of the selected candidates. Therefore, the candidates are advised to check the result page thoroughly and if there is any requirement mentioned against their name, they should submit the documents asked for, at the earliest possible at the BSPHCL office.
The Bihar State Power Holding Company Limited (BSPHCL) had invited applications to recruit Assistant Operator, Switch Board Operator-II, Junior Line Man, and Technician GR-IV in the month of September-October 2018. As per the notification there were around 2050 vacancies to be filled through the examination.
What type of work do technology engineers perform?
4 What type of work do technology engineers perform?


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Study reveals the average duration of a sex session
Miley Hayden 2 years ago
You'd be forgiven for thinking that we humans do nothing but talk about sex. But even when us amorous apes actually stop doing the jaw-jaw and get down to business, there's still one question haunting our horny brains: just how long should sex last?
If you're Sting or Puff Daddy, you'd probably say sex should go on for at least the length of a bank holiday weekend. Whilst if you're an inexperienced spotty teenager, you'll probably be delighted if the time taken to complete a dirty deed matches the duration of an average Ariana Grande tune.
Now science has weighed in (again) to tell the world exactly how much time they should be spending in the act of physical love: 5.4 minutes.
"If you're a non-scientist, you might have once asked yourself, propped against the bedhead after disappointingly quick intercourse, how long does sex 'normally' last?" Dr Brendan Zietsch from the University of Queensland wrote in The Conversation .
"A scientist, though, would phrase the same question in an almost comically obscure way: What is the mean intravaginal ejaculation latency time?
"I know there's a lot more to sex than putting the penis into the vagina and ejaculating, but the rest is not always easy to define (kissing? rubbing? grinding?).
"To keep things simple and specific, we'll just focus on the time to ejaculation."
Dr Brendan Zietsch recounted a study in which 500 couples were armed with a stopwatch and asked to press the button (of the clock) when the unspeakable act begun and then tap it again when the man experiences his magical moment. "That is as practically awkward as it sounds: participants pressed 'start' at penile penetration and 'stop' at ejaculation," he added.
"You may note this could affect the mood somewhat, and might perhaps not exactly reflect the natural flow of things.
"But science is rarely perfect, and this is the best we've got."
This study found that sexy time lasts anywhere between 33 seconds and 44 minutes, with the median time coming in at 5.4 minutes. Interestingly, the research also explores "conventional wisdom regarding penile sensitivity and its relationship to staying power in the sack".
Older men weren't able to last longer than young ones, while wearing a condom or being circumcised didn't boost chaps' performance either.
"Another surprising finding was that the older the couple, the shorter the sex, contrary to the prevailing wisdom (probably peddled by older men)," Zietsch continued.
via – THESUN UK
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Miley Hayden is a staff writer for FunkPost and is based in Israel. Miley Hayden is a Reporter by profession, covering viral content, Internet culture and Trending Topics.
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redpajama_set_name: RedPajamaCommonCrawl


text:
Where to watch the Oscars
Catch all the excitement of the 88th annual Academy Awards at one of these Oscar viewing parties in and around Boystown, Chicago.
The 88th annual Academy Awards, which will be held at the Dolby Theatre in Hollywood, Sunday, Feb. 28, will air live on ABC. The telecast begins at 6:00 p.m. CT, and starts with the red carpet. The ceremony will be hosted by Chris Rock.
On the Red Carpet: A Night with Oscar
The Center on Halsted welcomes donors, patrons, and supporters to enjoy the Academy Awards presentation in a fun and festive atmosphere…. it's On The Red Carpet: A Night with Oscar beginning at 6 p.m.
2/28/2016 | more info about this event in the calendar
Watch the Oscars on the Sidetrack Big Screen
Watch the Oscars at Sidetrack... on all screens, including the Big Screen in Main Bar. Warm up before with Show Tunes starting an hour earlier than usual at 3pm and then cap off your Sunday Funday with The Academy Awards, hosted by Sidetrack's own Dixie Lynn Cartwright and her sexy movie ushers.
Kit Kat's Academy Awards Viewing Party
Kit Kat rolls out the red carpet for the Academy Awards. All seven HD projection screens will be tuned in to Hollywood. Diva Dulce Andrews will entertain the crowd with live performances. Kit Kat's theatrical-themed dinner menu will be served.
Oscars @ the Twisted Vine
Come dressed to impress at the Twisted Vine Oscars viewing show with specials on mini dogs, champagne and old fashions with complimentary popcorn flowing all night long.
Oscars at Atmosphere
Atmosphere Bar is having an Oscars party and you're invited. Oscar voting ballots with prizes for the winners, multiple screens, full sound, drink specials and more.
Oscars Viewing Party
Watch the Oscars with the men of Touche' during the Beer Bust. Show starts at 6PM.
Slave 4 Britney Sundays: Oscars Edition!
Roscoe's Tavern presents a night dedicated to the Princess Of Pop & Living Legend - Britney Spears. In honor of the Academy Awards this will be a very special Oscars edition of Slave 4 Britney Sundays!
Hollywood on State: When You're the Star
The Gene Siskel Film Center (GSFC) of the School of the Art Institute of Chicago (SAIC) hosts Chicago's longest-running awards show viewing party, "Hollywood on State: Where You're the Star."
Oscars at The Call
Watch the Oscars this Sunday at The Call Bar. No Cover.


If you're looking for a low priced, powerful and reliable crossbow the Ballistic-370 is ideal for you. It's high quality aesthetics and unique ergonomic features make it a top buy for anyone wanting to do some target shooting.
Built to last the Ballistic come with and aluminium / composite barrel offering a balanced weight and durable crossbow. This barrel is then fitted with a picatinny rail to allow accessories such as optics, lasers and torches to be attached. The riser is bade from an aluminium die casting to then further this even more.
Fitted with a stock built from reinforced composite this crossbow is extremely accurate. The stock is adjustable allowing you to chance it according to your shooting position. To then further the accuracy of this crossbow even more the Ballistic has an AR grip for a solid hold over your equipment. To prevent damage to your crossbow and prolong it's life the ballistic has an anti-dry fire trigger preventing you shooting when no bolt is loaded.
The Ballistic ensures smooth cycling for clean cocking and shooting. It achieves this by having CNC cut cams with a high quality finish. To then further the shooting power and quality of this crossbow the Ballistic 370 has compressed fiberglass limbs for durability and accuracy. One of the nicest features on this crossbow is the extended bullpup trigger. This pushes the grip forward helping to compact the crossbows designs and results in a more balanced and ergonomic crossbow.
Alongside This powerful, accurate crossbow you get a handful of accessories to get you started including a 4x32 scope, cocking rope, shoulder sling, 3-bolt quiver, 3 x 20" Carbon bolts and string wax.
Speed: 370fps Draw Height: 185lbs Power Stroke: 13.75" Axle To Axle: 18" uncocked Weight: 6.7lbs Length: 34.5"-37"


Thanks to cooperation with world-renowned Korean electronics manufacturer, FIBARO devices have been integrated with one of the most popular IoT platform, namely the SmartThings. Such a connection enables associating FIBARO devices with other manufacturers equipment based on Samsung platform.
Samsung SmartThings is currently one of the most recognized Internet of things platforms in the industry. Manufacturers have the opportunity to offer their customers equipment that works not with one but with many brands, which will allow even better use of the smart home potential in everyday use.
Cooperation with Samsung and the presence of FIBARO products on the SmartThings platform gives practically unlimited possibilities of expanding the system with functionality provided by FIBARO devices. This kind of integration is a great enterprise, benefiting both, the manufacturers and their users. The SmartThings platform is present in more than 200 markets worldwide. This gives a unique opportunity to expand and offer FIBARO products to new customers. We must not forget about the constantly growing market of domotic solutions, the increasing user requirements and telecom projects which is why it is so important for us to enter into cooperation with Samsung.
– explains Krzysztof Banasiak, the Member of the Board at FIBARO.
Thanks to the integration of FIBARO devices with SmartThings, the possibilities of a smart home had become significantly expanded. Users benefit from additional features in areas such as safety, entertainment, lighting and HVAC. For example, when the FIBARO Motion Sensor detects movement in a room, it automatically adjusts the heating or cooling of the interior simultaneously, thanks to the presence in a smart watch manufactured by SmartThings – an appropriate notification of this fact will be displayed on the watch. Another useful feature is the control of electricity consumption by means of micro modules and the Wall Plug integrated with the SmartThings platform which enables detailed savings report to improve any home budget.
By combining the possibilities offered by FIBARO and Samsung, the user will also be able to control the household appliances of this brand, thus offering even wider possibilities of operation and use of these products on a day-to-day basis.
The possibilities of the system are so great that we will be limited only by our imagination. It is possible that the nearest future will enable turning on heating in the car, check the fuel, oil or tyre pressure via the app. You can already find Tesla or Subaru among the brands integrated with SmartThings. We believe that further development of this platform and other projects implemented with SmartThings by Samsung is moving forward very dynamically, I am glad that FIBARO is an integral part of these changes.
Keep in mind that the list is still expanding and you can see new smart home products compatible with SmartThings in a short time.


DHAKA | NEW DELHI: South Asia is one of the most sensitive regions with regard to impact of climate change, India said today and called for SAARC countries to cooperate in addressing its impact on the farm sector.
areas under the control of Indian Railways, airports, airbase, port and harbour, defence establishments,special economic zones, State and Central government organizations, places of pilgrims, religious & historical importance.
began to resemble an election rally. Fairly so, for locals say the white tiger has been an election issue here for years now.
NAGPUR: PTI The Centre has planned to introduce tree farming in India to increase the forest cover in the country, Union environment and forests minister Prakash Javdekar said here on Sunday.
BHOPAL: Madhya Pradesh has lost nearly 16 tigers, including seven in Pench reserve, due to poaching and others reasons in the last one year.
While an NGO blamed the state government for it, forest officials contended that most of the deaths were natural.
The Karnataka Forest Department (KFD) has decided that the best way to curb man-elephant conflict in the Rajiv Gandhi (Nagarahole) Tiger Reserve area is to clear out 10,000 acres of teakwood trees and replace them with fruit-bearing ones.
What's more, the decision has even garnered nods from elected representatives of the Kodagu and Mysuru regions.


In the present dearth of coal, it is satisfactory to know that efforts are being made in various directions to meet the public wants in the way of fuel. We have heard good deal lately of processes for the utilisation of peat —a substance which commends itself once in respect of its abundance, and of its richness in burning material. It has been generally felt that if the substance forming our vast moors could be converted into a fuel equal or nearly equal to coal, the question which has been causing so much anxiety to householders and manufacturers would be practically solved, while a new source of wealth would be opened up in districts hitherto comparatively unproductive. The difficulty to be overcome in the first instance was to devise a method of preparation which should give the peat the necessary solidity and heating power.
Among those who have turned attention to the subject is the Duke of Sutherland, a nobleman whose intelligent interest in all schemes of improvement adds additional lustre to his rank, and who, of course, is fully alive to the importance of any enterprise which promises indefinitely to enhance the value of moorland property. For some time past the Duke has been experimenting, with more or less success, in the preparation of peat by compression.
Latterly, however, his Grace has become connected with an undertaking which, by means of a more elaborate process, aims at the conversion of peat and coal waste into a fuel capable of meeting all requirements. We refer to a patent recently taken out by Mr Pender, M.P., for set of machinery contrived, we believe, by his factor, Mr Rae, with reference to system of fuel manufacture which presents some features novelty. For the working of this patent, a company is in course of formation, with the Duke of Sutherland at its head, and operations are about to be commenced at Seafield, near Bathgate, where, as well as in the adjacent property of Blackburn, leases of coal, shale, and peat have been obtained from Mr Pender.
The process in question is adapted for the production of two, it may be three or four varieties of fuel, the materials employed being coal dust, peat, crude shale oil and shale tar, or other similar substance. One compound proposed to be made is that of coal dust and tar; another will consist of peat and tar, with a certain admixture of oil. Or the coal dust fuel may be mixed with oil with a view to the production of gas-making material, or, again, it may be found desirable to mix coal-dust and peat in certain proportions. important feature of the process is the mode of preparation the tar, for which a portion of the machinery designed Mr Rae is specially appropriated. The tar is first steamed and washed with lime water, so as to extract any acid it may contain, after which, by the removal of a certain portion of oil, it is reduced to the condition of a mastic, or something of a consistency between tar and pitch. In this state it can be used in smaller quantity, and gives to the fuel made with it a toughness and solidity not to be attained by the use of pitchy substance.
Other portions of the machinery provide for the crushing of coal and the maceration of peat, the thorough drying those substances after having been so dealt with, and the subsequent mixing of them with tar or oil. The compound thus formed is next subjected to pressure, and having been cut into blocks, is delivered in that state upon a creeper or endless web, by which it is carried away from the machine, and by which, if thought necessary, it may be carried through a furnace and subjected to a process of roasting, with the view of rendering the surface impervious to atmospheric influences.
The fuel produced in this way has, we are told, been subjected to variety of tests, and with such results as seem to augur well for its general adoption. In regard to its capability for standing exposure to the weather, it appears that a quantity made at Dunrobin lay uncovered during the whole of last winter without deterioration. The question whether it is equally adapted to resist disintegration by heat is now being put to the test of experiment. The coal dust fuel, which consists of coal and tar in the proportion of 93 to 7, is found to be so compact that something like 90 tons can be stowed in the space occupied by about 50 tons of coal. In regard to other qualities, it has been tested the Admiralty at Portsmouth Dockyard, with satisfactory results ; and trial has also been made of it in railways and steamboats. Among other recommendations, it turns out to be particularly well adapted for the rapid raising of steam. Then again the amount of ash produced is so trifling that very little stocking is required ; and as for heating power, practical men will understand the value of a fuel which claims to have evaporated 9| lb. of water for each pound consumed. The peat fuel, which, in addition to tar, contains from 5 to per cent, of oil, has come out equally well in experimental trials. Whereas the condensed peat prepared at Dunrobin could only be got to evaporate lb. of water per pound consumed, the peat fuel produced by the process just described was found, when tested the Duke's railway, to have an evaporating power of lb.
Duke Sutherland's property at Brora. In that quarter there is peat ad libitum, together with plenty of shale and coal. The shale, of which two thick seams have been proved, is found to yield a very high percentage of oil, and that of a density which renders it peculiarly suitable for the production of tar. The coal was worked as early as Queen Elizabeth's time, but has been entirely neglected for the last fifty or sixty years. Now, however, there seems every probability of that, well as the other mineral wealth of the district, being turned to profitable account.— Scotsman.


text:
import jwt from 'jsonwebtoken';

/**
 * @class EnsureToken
 */
export default class EnsureToken {
/**
 * This method is used to validate users token
 * @param {obj} req
 * @param {obj} res
 * @param {obj} next
 * @return {json} Returns request object containing message of
 *  if request is granted or denied
 */
  static token(req, res, next) {
    const token = req.body.token || req.query.token || req.headers['x-access-token'];
    if (token) {
      jwt.verify(token, process.env.SECRET_KEY, (err, decoded) => {
        if (err) {
          return res.json({ success: false, message: 'Failed to authenticate token.' });
        }
        req.decoded = decoded;
        next();
      });
    } else {
      return res.status(403).send({
        success: false,
        message: 'Access denied. Login first'
      });
    }
  }
}

redpajama_set_name: RedPajamaGithub


text:
Public Input on Mello Station Closed
by Stewart Lytle
The controversial intersection of East Main Street and Carleton Drive. Photo credit: Stewart Lytle / Town Common Media
GEORGETOWN – After more than a year and a half of gathering information about G. Mello Disposal Corp.'s proposed new 500-ton transfer station, the town's Planning Board last week abruptly shut down its fact-finding effort and moved to deliberate at its next meeting on what conditions the town will impose on the large trash collection company.
Mello agreed prior to last week's meeting that it would limit its operation at the new station to 200 tons during the first year and increase the tonnage each year for four years to reach the 500-ton capacity.
The board, which can only regulate the "layout, scale, appearance, safety and environmental impact" of the proposed transfer station on Carleton Road near Interstate 95, will begin deliberations on the new station on Sept. 8.
It was also disclosed at this hearing that Mello has offered no host agreement to benefit Georgetown and cover additional expenses it may cause the taxpayers. Host agreements are common in towns for large projects and are required for recreational marijuana sales.
According to Mike Birmingham, an opponent, the town of Holbrook receives almost $1 million a year from its host agreement with a transfer station.
Mello's proposal, which has drawn substantial resident opposition, faces scrutiny by other town boards and officials, including the Conservation Commission, which postponed its consideration of the transfer station until its next meeting.
The transfer station must also secure a building permit from Angelo Salamone, the town's building inspector, who could decide that the town's new bylaw limiting transfer stations to 50 tons would prevent him approving a 500-ton transfer station. The bylaw was approved by the Attorney General, but the town adopted it after Mello filed its application to build the large station. That issue would certainly be litigated in court.
Last week after about two hours of discussion, including comments from dozens of residents, Planning Board vice chair Bruce Fried proposed to close the public hearing. It was seconded by Joanne Laut.
A surprised Robert Watts questioned whether Fried knew his motion would prevent the board from gathering more information from the public on the project. Fried said he did. Town Planner John Cashell explained to the board that if it approved Fried's motion, it would begin deliberations on the project at its next meeting.
Despite those warnings, the four-member board voted unanimously to end the public hearing.
Board member George Comisky, who has recused himself from voting on the Mello project, said he believes the town needs more information about the project.
Harry Cortiglia, the Planning Board chair, told the board that once it issues a site plan approval, "there's very little the board can do."
A major focus for the Planning Board will be traffic on Carleton Drive and its intersection with Rte. 133 (East Main Street). Mello has promised to hire an off-duty police officer for the first 60 days to help manage the flow of traffic at the intersection.
Board member Bob Watt said he found "very credible" the videos Jon Samel, an opponent who operates two businesses on Carleton Drive The videos showed trucks crossing the centerline of Carleton Road and blocking the intersection with the state highway. Mello produced videos showing trucks easily making the turn to and from Carleton Drive.
Mello's proposal to limit the tonnage during the first five years included a review of the transfer station operations by the Planning Board before it allows Mello to increase the tonnage for the next year. It was unclear what authority the board has to force Mello to make changes, if it decides some are needed.
Fried said the board must have the authority to stop the transfer station operations as part of that review. "This is a huge project. If we don't get this right, we can't go back and fix it," Fried said.
The site of the proposed 500-ton transfer station. Photo credit: Stewart Lytle / Town Common Media
Who will pay to reconstruct Carleton Road is another issue, but that will be decided by the Board of Selectmen, which has the authority to decide if and how much money Mello will have to pay to rebuild the narrow access road to the station.
Engineers, after analyzing numerous borings in Carleton Drive, concluded that the narrow road with a thin top of asphalt and poor drainage must be rebuilt to sustain the impact of hundreds of trucks and cars per day using the transfer station.
Mello attorney Nancy McCann told the board the company has been discussing rebuilding Carleton Drive with town highway surveyor Peter Durkee. Town Planner John Cashell said Durkee told him he "is amenable to working with Mello to reconstruct the road."
The Planning Board was given no details.
Sixty people attended the hearing. Of those, dozens of residents opposed the project. Theodora Capaldo said, "We are trying to fit a very large square in a small hole." She also questioned why no other municipality is trying to take this transfer station from Georgetown. "If it was good for a community, other towns would be competing for it."
Samel said the traffic studies presented to the board are not accurate. He recently did his own survey and found that about 180 vehicles per day use Carleton Drive. Once the station is in operation, the proposed number of vehicles will be much higher.
Former Selectman Steve Sadler said the town's bylaws prohibit intersections being rated as an F and require that the town bring them up to at least a D rating. The intersection at Carlton Drive and Rte. 133 is rated at F and is expected to be worse when the transfer station is operating.
"It is going to be a horrible situation," Sadler said.
Several neighbors said they were just finding out about the proposed station and were outraged that the town is considering it. Kathy Birmingham, a long-time opponent of the station, said, "My heart breaks for those people who are only now learning about this project."


Elevate your bedroom decor with the Positano Bed. A series of wide, plush velvet upholstered segments rise and fall to create the striking main design element of this bed. The look is completed with an upholstered platform base and lucite block legs. Customizable velvet allows you to perfectly match any room.
Dimensions: Vary depending on bed size.


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La Force [] (okzitanisch: La Fòrça) ist eine französische Gemeinde mit  Einwohnern (Stand: ) im Département Dordogne in der Region Nouvelle-Aquitaine. Sie gehört zum Arrondissement Bergerac und zum Kanton Pays de la Force. Die Einwohner werden Forcelais genannt.

Geographie
La Force liegt in der Landschaft Périgord am Fluss Dordogne, der auch die südliche Gemeindegrenze bildet. Im nördlichen und westlichen Gemeindegebiet verläuft sein Nebenfluss Eyraud. Umgeben wird La Force von den Nachbargemeinden Saint-Georges-Blancaneix im Norden, Prigonrieux im Osten, Lamonzie-Saint-Martin im Süden sowie Saint-Pierre-d'Eyraud im Westen.

Bevölkerungsentwicklung

Sehenswürdigkeiten

 Schloss La Force, in den Jahren 1604 bis 1614 für den Herzog von La Force im Stil der Renaissance errichtet, wurde um 1793 zerstört. Die Ruine diente als Steinbruch. Von der Schlossanlage erhalten geblieben sind das Henkelbogenportal, Teile der Fassade und die Durchfahrt des Eingangspavillons der früheren Stallungen, auch Pavillon des récettes genannt. Er steht seit 1932 als Monument historique unter Denkmalschutz.
 Die protestantische Pfarrkirche (Anfang 17. Jahrhundert), die dem Pavillon des récettes benachbart ist, wurde ebenfalls unter dem Herzog von La Force als damalige Schlosskapelle errichtet. Da ihr Auftraggeber   calvinistischen Glaubens war, diente sie bis zur Widerrufung des Ediktes von Nantes (1685) auch der protestantischen Pfarrgemeinde. Ihre Zerstörung konnte durch eine Zurückstufung zur Schlosskapelle verhindert werden. Das Gebäude wurde 1806 von Protestanten erworben und 1821 restauriert.
 Die protestantische Kirche der John-Bost-Stiftung ist weiter westlich an der Rue du Pasteur Alard zu finden.
 Die katholische Pfarrkirche Saint-Victor, deren Bau 1865 beschlossen wurde, erhebt sich am Standort einer Vorgängerkirche. Sie wurde 1874 geweiht und bewahrt eine Reliquie des heiligen Viktor von Marseille.

Persönlichkeiten
 Jacques Nompar de Caumont (* 1558; † 1652 Bergerac), seigneur de Castelnau, 1. duc de La Force und Pair von Frankreich (1637), Marschall von Frankreich (1622)
 Armand Nompar de Caumont (* ~1580/1582; † 1675 Schloss La Force), ältester Sohn von Jacques Nompar Caumont, 2. duc de La Force und Pair von Frankreich (1652), Marschall von Frankreich (1652)
 Henri Nompar de Caumont (* 1582 Schloss La Force; † Januar 1678 ebenda), zweiter Sohn von Jacques Nompar Caumont, marquis de Castelnau, 3. duc de La Force und Pair von Frankreich (1675)
 Jacques Nompar II de Caumont (* 1632; † 1699), Enkel von Henri Nompar, baron de Boisse, 4. duc de La Force und Pair von Frankreich (1678)
 Henri François-Xavier de Belsunce de Castelmoron (* 1671 Schloss La Force; † 1755), Bischof von Marseille
 Henri Jacques Nompar de Caumont (* 1675; † 1726 Paris), Sohn von Jacques Nompar II, 5. duc de La Force und Pair von Frankreich, Mitglied der Académie Française
 Armand Nompar II de Caumont (* 1679; † 1764 Schloss La Force), Bruder von Henri Jacques Nompar, 6. duc de la La Force und Pair von Frankreich
 Anne-Jacobé de Caumont (* 1758 Schloss La Force; † 1842), comtesse de Balbi
 Ami Bost (* 1790; † 1874 La Force), evangelischer Pfarrer
 John Bost (* 1817; † 1881), evangelischer Pfarrer

Weblinks

Anmerkungen und Einzelnachweise

Ort in Nouvelle-Aquitaine

redpajama_set_name: RedPajamaWikipedia


There's a clear difference in Queen Letizia of Spain's style from the moment it was first announced that the TV reporter (then known as Letizia Ortiz) was engaged to Prince Felipe, back in 2003, to today. During her first years as princess of Spain, Letizia kept a conservative look, wearing pantsuits, high necklines, and demure gowns, much like she did during her journalist days. But in the past couple of years, the queen has taken more risks, giving her style a modern turn in body-hugging dresses, printed skirts and pants, and Disney-worthy gowns. See the royal's transformation ahead, then check out her best moments with the king.


HIV infects and propagates into CD4+T lymphocytes and macrophages, although many other cell types play an important role in virus spreading and pathogenesis. In addition to regulatory viral proteins, the cytokine network has early been implicated as a major controller of the plastic capacity of HIV to spread productively or rather remain silently integrated in the chromosomes of infected cells. The recent discovery of CCR5 and CXCR4 as essential entry co-receptors together with CD4 has highlighted a novel and potentially important step in the pharmacological hunt for more effective antiviral agents. In addition to regulate HIV expression and replication, several cytokines have demonstrated the capacity of up- or down-modulating chemokine receptors including CCR5 and CXCR4 with the consequence of influencing the susceptibility of T cells and macrophages to HIV infection. Pharmacological agents such as pertussis toxin B-oligomer have demonstrated HIV suppressive effects via non competitive binding of CCR5, whereas interferons or interleukin-16 (IL-16) can prevent post-entry steps in HIV expression. At the clinical level, several cytokines or their receptors are useful markers for monitoring disease progression and its consequence on the immune system. Cytokine-based therapy represents a realistic complementary approach to traditional antiretroviral therapy potentially capable of restoring important adaptive or innate immune functions ultimately curtailing HIV spreading and its consequences on the immune system, as exemplified by the experimental clinical use of IL-2.
Abstract: HIV infects and propagates into CD4+T lymphocytes and macrophages, although many other cell types play an important role in virus spreading and pathogenesis. In addition to regulatory viral proteins, the cytokine network has early been implicated as a major controller of the plastic capacity of HIV to spread productively or rather remain silently integrated in the chromosomes of infected cells. The recent discovery of CCR5 and CXCR4 as essential entry co-receptors together with CD4 has highlighted a novel and potentially important step in the pharmacological hunt for more effective antiviral agents. In addition to regulate HIV expression and replication, several cytokines have demonstrated the capacity of up- or down-modulating chemokine receptors including CCR5 and CXCR4 with the consequence of influencing the susceptibility of T cells and macrophages to HIV infection. Pharmacological agents such as pertussis toxin B-oligomer have demonstrated HIV suppressive effects via non competitive binding of CCR5, whereas interferons or interleukin-16 (IL-16) can prevent post-entry steps in HIV expression. At the clinical level, several cytokines or their receptors are useful markers for monitoring disease progression and its consequence on the immune system. Cytokine-based therapy represents a realistic complementary approach to traditional antiretroviral therapy potentially capable of restoring important adaptive or innate immune functions ultimately curtailing HIV spreading and its consequences on the immune system, as exemplified by the experimental clinical use of IL-2.


Free Shipping in the continental US (lower 48 states) This package include both front and rear 2004-2015+ STi or 03-15 Evo Project Mu B-Force Pads.
A step up from Project Mu's Type NS, these pads still provide excellent street driving characteristics. They still provide minimal dust, noise and rotor wear, but these will also stand up to autocross and light track duty. These are a great compromise for those looking for a performance pad without lots of dust and noise.


It's that time of year once again where you, the Sleaze Roxx Readers, determine which were the best albums of the year for the 13th straight year.
CAST YOUR VOTE VIA E-MAIL TO: oliviersleazeroxx@yahoo.com.
Just like in previous years, please submit your top five CDs of the year in order from top to bottom (one to five). Five points will be awarded for each number one entry, four points for each number two entry and so forth until the fifth entry is reached which will be awarded one point.
Albums including EPs (three songs or more) must be released in 2018 to be eligible. Live albums, greatest hits and re-issues are not eligible.
You have until January 11, 2019 to vote and you can only vote once per e-mail address.
The Sleaze Roxx's Top Ten Albums of 2018 will be posted sometime in the morning of December 31, 2018.
The Sleaze Roxx Writers' Top Five Albums of 2018 will be posted in early to mid-January 2019.
In the meantime, you can check out last year's Sleaze Roxx Readers' Top 20 Albums of 2017.


text:
Anti-Bias Leaders ECE
With Louise Derman-Sparks, Debbie LeeKeenan, John Nimmo
Louise Derman-Sparks
Debbie LeeKeenan
John Nimmo
Reflecting on Anti-bias Education in Action: The Early Years
The Voices of Children
Tools, Resources, Links
Anti-Bias Pledge
A director's book: From Survive To Thrive
Leadership Retreats in Italy
Social Justice Retreat 2016
Childcare Exchange
Film – Reflecting on Anti-bias Education in Action: The Early Years
Reflecting on Anti-bias Education in Action: The Early Years, is a 48 minute film that features vignettes of anti-bias strategies in early childhood classrooms interspersed with teachers reflecting on their practice. A facilitator and viewer guide is available in English and Spanish. The film has received numerous awards including the Silver Prize for Documentary Feature (2021) in the Social Justice Film Festival and a nomination for Northwest Regional Emmy® (2022) in the category of diversity, equity, and inclusion – long form content.
Stream film here
Purchase DVD and guide book here
Debbie LeeKeenan and John Nimmo produced the film which was released April 2021 for free streaming. They partnered with filmmaker Filiz Efe McKinney of Brave Sprout Productions to create a film that shifts the focus away from the talking heads of experts and on to the voices of teachers committed to equity on a daily basis. By taking viewers into diverse ECE classrooms, the film seeks to demonstrate the importance of teacher reflection on identity, context, and practice in anti-bias education and provides a much-needed resource for teacher education and professional development. Here is a blog post.
Louise Derman-Sparks is the film's senior advisor. The film's theoretical and research framework is based on her co-authored books, Anti-Bias Education for Our Children and Ourselves (with Julie Olsen-Edwards and Catherin Goins ) and Leading Anti-Bias Early Childhood Programs: A Guide for Change (with Debbie LeeKeenan and John Nimmo).
Latest news about the film * Awards and Festivals
Equal rights, fair play, justice are all like the air-we all have it or none of us have it.
-Maya Angelo, Academy of Achievement Interview
Anti-bias education is a commitment to supporting children who live in a highly diverse and yet still inequitable world. It is an underpinning perspective and framework that permeates everything in early childhood education. We stand committed to nurture a more diverse and inclusive generation of young children who thrive through their experience of equitable learning opportunities in early learning programs. We aim for each child to demonstrate self-awareness, confidence and family pride and positive social identities, express comfort and joy with human diversity, to increasingly recognize injustice, and to have the will and the skills to act against prejudice.
Our writing, including our 2015 book, Leading Anti-Bias Early Childhood Programs – A Guide for Change, our presentations, and our consultation services draw on many years as teachers, teacher educators and researchers, social justice activists, and leaders of early childhood programs. On this site you will find some background into who we are and the resources we have developed.
We also invite you to share your experiences with leading anti-bias change in your own early childhood or teacher education program and in implementing the ideas and strategies that we offer on this site and in our publications.
— Louise, Debbie and John
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text:
Aguiar da Beira est une ville et municipalité (en portugais : concelho ou município) du Portugal située dans le district de Guarda et la région Centre.

Géographie
Aguiar da Beira est limitrophe :
 au nord, de Sernancelhe,
 à l'est, de Trancoso,
 au sud-est, de Fornos de Algodres,
 au sud-ouest, de Penalva do Castelo,
 à l'ouest, de Sátão.

Histoire
La charte – foral, en portugais – de la municipalité a été octroyée en 1120 par Thérèse de León (1080-1130), comtesse régente de Portugal.

Démographie

Jumelages

Subdivisions
La municipalité d'Aguiar da Beira groupe 13 paroisses (freguesia, en portugais) :
 Aguiar da Beira
 Carapito
 Cortiçada
 Coruche
 Dornelas
 Eirado
 Forninhos
 Gradiz
 Pena Verde
 Pinheiro
 Sequeiros
 Souto de Aguiar da Beira
 Valverde

Voir aussi
 Villes du Portugal
 Liste des municipalités du Portugal

Liens externes
 Photographies d'Aguiar da Beira

Notes et références

Municipalité au Portugal
Ville au Portugal
District de Guarda


text:
Home General More demolition of illegal structures at Glefe
More demolition of illegal structures at Glefe
By Josephine Akari & Emmanuella Jackson.
Victims of the demolition exercise carried out at the Gbugb3 Lagoon at Glefe, a suburb of Dansoman in Ablekuma West, have accused the Municipal Authority of not giving them ample time to gather their valuables. They complained that a similar exercise was carried out about three years ago, to protect the lagoon and the sea, but since that exercise, nothing had been done to save the situation. They added that the Covid-19 pandemic has negatively affected the economy and caused hardship to many Ghanaians, therefore, pulling down their homes was the most inconsiderate thing to do, especially as the festive season is approaching.
Checks by GBC News at the demolition site indicated that about 300 structures, including Schools and a Church were pulled down.
At the time of the visit, some of the victims were gathered at the site and one could tell they were still in shock.
According to them, they were given the quit notice on the 10th of November, 2021, but they pleaded with the Assembly for more time which did not yield any result.
The affected persons mentioned that they have not been treated fairly as they pay electricity and water bills and therefore had equal rights just like other residents.
"We don't have money to rent. My mother arrived yesterday and she had to be compelled to sleep outside. The rains do not affect us in any way for them to carry out this demolition. We all wish we could live in East Legon, but for lack of money", a resident lamented.
" We were only given two weeks prior notice. The Tenancy Agreement gives three months prior notice for eviction so why were we given only two weeks. We could not gather any belongings. The Police were present to sack us from our rooms so we couldn't take a penny. The excavators destroyed everything. In this Covid era, how can you eject someone within three weeks", another resident questioned.
While the affected people counted their loss, some scrap dealers saw it as an opportunity to scavenge for metals.
Jennifer Lawrence engaged to art gallery director Cooke Maroney
Mixed reactions trail survey on Election 2020
South Africa to reopen places of worship


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text:
Managing Director, Head of Technology Mergers & Acquisitions
Technology Investment Banking
Chairman of the Fairness Opinion Review Committee
Peter Lombard is a managing director in the technology investment banking group, heads the technology M&A team and chairs the fairness opinion review committee at Piper Jaffray.
Lombard has more than three decades of investment banking experience with a primary focus on M&A in technology, tech-enabled services, information and marketing services, and healthcare. Recent transactions include representing DentalPlans.com in its sale to Internet Brands, Innocoll Plc in its sale to Gurnet Point Capital, Medtronic Plc in the divestiture of its Patient Recovery Business to CardinalHealth, AuthenTec in its sale to Apple; Stratasys in its merger with Tel Aviv-based Objet Ltd., C Space in its sale to Omnicom, and Switch & Data Facilities Company in its merger with Equinix Inc.
Prior to joining Piper Jaffray in 2008, Lombard was a managing director in the M&A group at Jefferies & Company. Previously, he headed Cowen & Company's M&A group and ran the Boston investment banking office of Robertson Stephens, where he also co-headed the M&A Group. He began his investment banking career in M&A at Merrill Lynch in New York City.
Lombard is a former independent board member of the SCS Hedged Opportunities Fund, LLC and a past member of the board of the Boston Philharmonic. He previously served three terms on the foundation board of the Massachusetts College of Art and Design, where he was vice chairman and treasurer.
Lombard received his bachelor's degree from Harvard College and a Master of Business Administration degree from Harvard Business School.
PeoplePublications and ReportsHighlighted TransactionsTransactions List


All requests for route changes, or changes of address or daycare, must come through the office of the school the child attends. The Transportation Department cannot accept requests for address changes or stop changes directly from any parent, daycare provider, or teacher. This is for the safety of the student and is intended to ensure that both the school records and the Transportation Department records are identical and correct.
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text:
Q: RightFax C# through RFCOMAPILib - Attachments I'm trying to send faxes through RightFax in an efficient manner.
My users need to fax PDFs and even though the application is working fine, it is very slow for bulk sending (> 20 recipients, taking abt 40 seconds per fax).
// Fax created
fax.Attachments.Add(@"C:\\Test Attachments\\Products.pdf", BoolType.False);
fax.Send();

RightFax has this concept of *Library Documents, so what I thought we could do was to store a PDF document as a Library Document on the server and then reuse it, so there is no need to upload this PDF for n users.
I can create Library Documents without problems (I can retrieve them, etc.), but how do I add a PDF to this? (I have rights on the server.)
LibraryDocument doc2 = server.LibraryDocuments.Create;
doc2.Description = "Test Doc 1";
doc2.ID = "568"; // tried ints everything!
doc2.IsPublishedForWeb = BoolType.True;
doc2.PageCount = 2;
doc2.Save();

Also, once I created a fax, the API gives you an option to "StoreAsNewLibraryDocument", which is throwing an exception when run. System.ArgumentException: Value does not fall within the expected range
fax.StoreAsNewLibraryDocument("PRODUCTS","the products");

What matters for us is how to send say 500 faxes in the most efficient way possible using the API through RFCOMAPILib. I think that if we can reuse the PDF attached, it would greatly improve perfomance. Clearly, sending a fax in 40 seconds is unacceptable when you have hundreds of recipients.
How do we send faxes with attachments in the most efficient mode through the API?

A: StoreAsNewLibraryDocument() is the only practical way to store LibraryDocuments using the RightFax COM API, but assuming you're not using a pre-existing LibraryDocument, you have to call the function immediately after sending the first fax, which will have a regular file (not LibraryDoc) attachment.
(Don't create a LibraryDoc object on the server yourself, as you do above - you'd only do that if you have an existing file on the server that isn't a LibraryDocument, and you want to make it into one. You'll probably never encounter such a scenario.)
The new LibraryDocument is then referenced (in subsequent fax attachments) by the ID string you specify as the first argument of StoreAsNewLibraryDocument(). If that ID isn't unique to the RightFax Server's LibraryDocuments collection, you'll get an error. (You could use StoreAsLibraryDocumentUpdate() instead, if you want to actually replace the file on the server.) Also, remember to always specify the AttachmentType.
In theory, this should be all you really have to do:

' First fax:
fax.Attachments.Add(@"C:\\Test Attachments\\Products.pdf", BoolType.False);
fax.Attachments.Item(1).AttachmentType = AttachmentType.aFile;
fax.Send();
fax.StoreAsNewLibraryDocument("PRODUCTS", "The Products");
server.LibraryDocuments("PRODUCTS").IsPublishedForWeb = BoolType.True;

' And for all subsequent faxes:
fax.Attachments.Add(server.LibraryDocuments("PRODUCTS"));
fax.Attachments.Item(1).AttachmentType = AttachmentType.aLibraryDocument;
fax.Send();

The reason I say "in theory" is because this doesn't always work. Sometimes when you call StoreAsNewLibraryDocument() you end up with a LibraryDoc with a PageCount of zero. This happens seemingly at random, and is probably due to a bug in RightFax, or possibly a server misconfiguration. So it's a very good idea to check for...
server.LibraryDocuments("PRODUCTS").PageCount = 0

...before you send any of the subsequent faxes, and if necessary retry until it works, or (if it won't) store the LibraryDoc some other way and give up on StoreAsNewLibraryDocument().
Whereas, if you don't have that problem, you can usually send a mass-fax in about a 1/10th of the time it takes when you attach (and upload) the local file each time.
If someone from OpenText/RightFax reads this and can explain why StoreAsNewLibraryDocument() sometimes results in zero-page faxes, an additional answer about that would be appreciated quite a bit!

redpajama_set_name: RedPajamaStackExchange


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A group of MPs have criticised the Scottish government's proposed foreign policy plans should they gain independence.
The world's "increasingly borderless" economy has helped rich individuals 'hide' over £12.5 trillion in offshore accounts, it has emerged.
David Cameron has spoken of his pride in Britain's role in removing Muammar Gaddafi from power, after confirmation of the renegade leader's violent death.
David Cameron lacks a cohesive foreign policy, according to the International Institute of Strategic Studies (IISS) thinktank.
Britain is prepared to launch another military intervention where circumstances permit, David Cameron has said.
When David Cameron shakes the hand of Chinese premier Wen Jiabao, he shakes the hand of a man who rules the world's largest remaining tyranny.
Violence in Syria has boosted Britain's hopes of securing a UN security council resolution against Bashar al-Assad's regime, politics.co.uk understands.
Russia is unlikely to shift its opposition to a resolution against Syria at the UN security council – however optimistic British diplomats may be.
Syrian president Bashar al-Assad's "vague promises" have been criticised by William Hague.
David Cameron's comments that Britain will keep the Falkland Islands have been dismissed as "mediocrity bordering on stupidity" by Argentina's president.
There is no obvious solution to the problems faced by the Liberal Democrats, Tony Blair has said.


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text:
Why Did Facebook Delete the 'Pray for Our President' Group? Interview with Donna Partow
December 4, 2020 October 19, 2020 by Kathryn Darden
Interview with Donna Partow: "Pray for Our President" Founder Donna Partow speaks out on the deletion of the popular prayer group by Facebook one month before the election
As reported yesterday, earlier this month, members of the 140k-large Facebook group "Pray for Our President," led by Christian author and speaker Donna Partow along with Carlos Sarmiento, noticed the group was no longer listed in their Groups list. Smaller groups with the same name remained, but the largest group dedicated to prayer and positive thought for President Donald Trump and other leaders had mysteriously vanished during the critical month right before the election.
What Happened to the "Pray for Our President Group" on Facebook?
Christian Activities did some research and discovered the group dedicated to praying for President Trump had been temporarily shut down by Facebook before. We reached out to founder Donna Partow to find out what had happened to the popular Facebook group, and she graciously agreed to answer our questions.
Interview with "Pray for Our President" Leader Donna Partow: Why Was the "Pray for Our President" Group Deleted?
CA: Thank you for allowing me to ask you some questions about the recent deletion of your successful Facebook group "Pray for Our President.
Donna Partow (DP): You are literally the first person who has actually cared about this as a "story." I've reached out to every Senator, Christian leader and political commentator I can think of. No response whatsoever.
CA: I think it is an important story and have wanted to get to the bottom of it. On your website, I read that the group was shut down in July. Then you were able to get it reinstated. When was it shut down the 2nd time?
DP: We were first deleted in July 2020, but after 4 hours on the phone with Facebook, I was able to have it reinstated.
We were suspended again in September, briefly, with no explanation. The group quickly returned with a notice from Facebook saying we had been deleted accidentally. "Oops. Sorry about that."
Our group was suspended on October 8th shortly before 1pm ET, when we were scheduled to go live with Republican congressional candidate, Madison Cawthorn.
CA: Did you have any warning from Facebook? What message did you receive when they deleted the group?
DP: We had no warning. We checked our "Group Quality" daily. If any posts were flagged by the supposedly "impartial" arbiters of truth, we deleted them, even if we disagreed with their determination We endeavored to keep a "clean" group with no violations.
We posted this multiple times per day:
The "Pray for Our President" Group Guidelines
CA: I saw your Trump Prayer Chain website. Do you have a new home on social media yet?
DP: No. Sadly, of the 140,000 members, only 4,000 provided their email address, so – if you factor in a 20% open rate on email – we would be basically starting from scratch.
CA: Why do you think your group was deleted by Facebook?
DP: It is obvious that we were deleted because we were EFFECTIVE, and we were making a difference. At our peak, we averaged 5,000 new members per day, thousands of daily posts and more than 100,000 comments per day. It was an extremely active group.
This was on a slow day:
Stats from a slow day for the Pray for Our President Group
Facebook shut us down because of our extensive pro-Trump reach on their platform.
Even now, if you type "pray for Biden" in the Facebook search bar, most of the results will STILL be…our Pray for our President group. That's how dominant we were.
CA: What else should our readers know?
DP: Facebook is a private company. If they are a "publisher" then they have every right to control what is published on their platform. My objection is that the are currently treated to the same legal protections as a utility company. But as my case clearly demonstrates, they are NOT functioning as an impartial utility that simply provides a neutral platform. They are clearly functioning as a publisher and should be subject to all of the same standards and guidelines of any other publishing company.
Facebook is clearly putting their thumb on the scales and pro-actively attempting to influence the coming election. Their efforts should be treated as in-kind political donations to the Biden campaign.
Publisher's note: Unfortunately, "Pray for Our President" is not the only conservative entity to be silenced on social media. Recently former Acting Director of National Intelligence Ric Grenell appeared on the Logan Sekulow ReProgram, claiming Twitter is censoring conservatives, and new free-speech social media platform Parler called last week the "worst week ever for social media suppression of information."
Social network platforms like Facebook and Twitter point to their "community standards" and TOS as reasons why conservative voices are silenced and groups are deleted, but they have no explanation as to why why BLM, Antifa, and other liberal groups are allowed to wish death and disease upon those with whom they disagree. Facebook and Twitter can interpret and apply their "community standards" however they see fit, because they are not accountable to anyone about their blatant efforts to control the flow of information to influence the 2020 election. Maybe it's time that kind of power was removed from social media platforms that choose to censor and control the opinions of their members.
Popular 'Pray for Our President' Facebook Group Deleted from Facebook
Parler Launches Erasebook.info to Expose Facebook's Deplatforming & Privacy Abuses; Facebook Immediately Blocks It
Conservatives, Christians, More Move to Social Networks USA.Life & Parler
Worst Week Ever for Social Media Suppression of Information
What Does the Bible Say About Politics?
Categories bytheway Tags Donald Trump, prayer, social networks 6 Comments Post navigation
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6 thoughts on "Why Did Facebook Delete the 'Pray for Our President' Group? Interview with Donna Partow"
Kevin A Connair
I agree wholeheartedly. This was anti-christian censorship at it's worst. The DOJ is beginning an anti-trust case against FB.
Good!!!
Susan Todd
I am sickened by Facebook censoring Christian thoughts, speech and prayers. Pray For Our President was a favorite of mine …I checked it every day, and read along with the wonderful prayers by so many Godly prayer warriors. I do pray that something can be done about Facebook and other social media's evil censoring! They certainly do not fear the LORD, OUR GOD
Kathryn Darden
Thank you for the comment about why the "Pray for our President" group disappeared from Facebook, Susan. I agree with what you said, and I also hope something can be done about social media censorship run amok.
Todd Engel
Thank you, Kathryn! I know the other 130,000 + members of Pray for Our President would send you many hugs for being a voice for them. Shame on Facebook. Hope they have to pay millions in damages (taxes) in the future. Todd E.
Thank you for the comment, Todd, and for bringing the matter to my attention. It is egregious that Facebook would delete a group whose intent was to pray for our President, that daily posted guidelines so in step with Facebook's community standards, and quickly deleted the few infractions they found. It is problematic that they shut it down with no explanation. Meanwhile, groups clearly devoted to overthrowing democracy, to harming authority figures like statesmen and police, that wish illness and death upon the President—these groups are allowed to flourish on Facebook. I hope something is done to penalize social media platforms that act like lackies for liberals by censorship of conservatives.


That's the miracle of babies, their ability to lay bare the tender, beating hearts of raging assholes.
I have to live the content, then come back and write about it.
I usually approach things with the idea that I will take something out of everything I do.
4 quotes by Heather Armstrong.


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