text:
\section{Introduction}
Since it is believed that majority of the stars in the Galaxy are formed in star clusters, the star clusters and their surroundings are important tools to study the star formation process. It is believed that star formation itself is a destructive process: as massive stars form in the region, their strong stellar winds and ultra-violet (UV) radiation immediately begin to disrupt the natal environment, consequently halting further star formation in the region. Alternatively strong UV radiation from massive stars associated with ionization front (IF) can trigger next generation star formation either through `collect and collapse process', which was proposed by Elmegreen $\&$ Lada (1977) or through radiation driven implosion (RDI) of a molecular cloud condensations. Detailed model calculations of the RDI process have been carried out by several authors (e.g., Bertoldi 1989, Lefloch $\&$ Lazareff 1995, Lefloch et al. 1997, De Vries et al. 2002, Kessel-Deynet $\&$ Burkert 2003, Miao et al. 2006). An observational signature of the `collect and collapse process' is the presence of a dense layer and massive condensations adjacent to  an {\mbox{H{\sc ii}~}} region (e.g., Deharveng et al. 2003), whereas observational evidence for RDI  process is often inferred from the spatial distribution of young stars and subgroups of OB associations and their age distribution (see e.g., Matsuyanagi et al. 2006, Sharma at al. 2007, Samal et al. 2007, Pandey et al. 2008).

In the RDI process a pre-existing dense clump is exposed to the ionizing radiation from massive stars of the previous generation. The head part of the clump collapses due to  the high pressure of the ionized gas and the self-gravity, which consequently leads to the formation of next generation stars. Thus one of the signatures of the RDI process is the anisotropic density distribution in a relatively small molecular cloud surrounded by a curved ionization/shock front. Bright-rimmed clouds (BRCs) are small molecular clouds located near the edges of evolved {\mbox{H{\sc ii}~}} regions and show the above signatures. So they are considered to be good laboratories to study the physical processes involved in the RDI process.

NGC 1893 is a very young cluster cluster (age $\sim$ 2-4 Myr) and a suitable object to study the star formation process. The cluster, located at the center of the Aur OB2 association, is associated with the {\mbox{H{\sc ii}~}} region IC 410. The cluster contains at least five O-type stars alongwith a rich population of pre-main-sequence (PMS) stars (see e.g. Sharma et al. 2007, hereafter S07). Several photometric and low resolution spectroscopic studies of the region have been carried out (for detail see S07; Prisinzano et al. 2011, hereafter P11). S07 and Maheshwar et al. (2007) have studied the star formation scenario around the NGC 1893 region. Although the studies by S07 and Maheshwar et al. (2007) reveal that stars lying away from the ionizing source are systematically younger;
 the fact manifesting a triggered star formation in the region, however, a question may be raised that the observed age sequence may be biased as those studies had used mainly classical T-Tauri stars (CTTSs) which either show a significant amount of H$\alpha$ emission and/ or NIR excess. On the basis of NIR $(J-H)/ (H-K)$ CC diagram the identification of weakline T-Tauri stars  (WTTSs) and CTTSs with small NIR excess is difficult as the NIR-CC diagram is significantly contaminated by the field star population (see e.g. Figure 16 of S07).

Recently, MIR $Spitzer$/IRAC and X-ray data from {\it Chandra} telescope have become available (cf. Caramazza et al. 2008, P11). Therefore, we considered worthwhile to re-investgate the star formation scenario in/ around of NGC 1893 region as well as to study the evolution of disk of TTSs in the NGC 1893 region using the newly available data.

\section {Data}

On the basis of optical, NIR, MIR and X-ray data P11 have identified 1034 and 442 Class II and Class III YSOs, respectively. We have used the optical and NIR data for the above mentioned YSOs given by P11. Whenever the NIR data for these sources are not available in the catalogue by P11, the same have been taken from the Two Micron All Sky Survey (2MASS) Point Source Catalog (PSC) (Cutri et al. 2003). Sources having uncertainty $\leq$ 0.1 mag (S/N $\geq$ 10) in all the three bands were selected to ensure high quality data. The $JHK_s$ data were transformed from the 2MASS system to the California Institute of Technology (CIT) system using the relations given in the 2MASS website.

\section {Distance to the cluster}

\begin{figure*}
\resizebox{12cm}{12cm}{\includegraphics{Fig1.eps}}
\caption{ $V_0/ (B-V)_0$  CMD for stars lying within  $r \le 3^{\prime}$ of NGC 1893 and having spectral type earlier than A0 (filled circles). The open circles are  the probable cluster  members (lying within $ r \le 10^{\prime}$)  identified by Eswaraiah et al. (2011) on the basis of polarimetry and photometry.  The isochrone of 4 Myr age (continuous line) by Girardi et al. (2002) corrected for the cluster distance is also shown. }
\label{fig1}
\end{figure*}

S07 estimated a variable reddening ($E(B-V) = 0.4 - 0.6$ mag) towards the direction of the cluster. Assuming a foreground reddening of $E(B-V) = 0.4$ mag, they estimated the distance to the cluster as 3.25 kpc using the $V/ (V-I)$ colour-magnitude diagram (CMD). P11 using a mean reddening $E(B-V) = 0.6$ and $V/ (U-B)$ CMD obtained a slightly higher value (3.6 kpc) for the distance. In our opinion the use of mean value of reddening is not appropriate to estimate the distance as it will yield a higher value to the distance.

Here we have re-estimated the distance to the cluster using the dereddened $V$ mag and $(B-V)$ colour. To avoid the contamination due to field stars we used the stars lying within 3 arcmin radius of the cluster. Reddening of individual stars having spectral types earlier than A0 has been computed by using the reddening free index $Q$ (Johnson \& Morgan 1953). Assuming a normal reddening law we can construct a reddening-free parameter index $Q = (U-B) - 0.72\times (B-V)$.
The value of $Q$ for stars earlier than A0 will be $< 0$. For main-sequence (MS) stars, the intrinsic $(B-V)_0$ colour and colour-excess can be obtained from the relation $(B-V)_0 = 0.332\times Q$  (Johnson 1966; Hillenbrand et al. 1993) and $E(B-V) = (B-V) - (B-V)_0$, respectively. Fig. 1 shows dereddened $V_0/(B-V)_0$  CMD for stars lying within 3 arcmin of the cluster center alongwith the probable members in the NGC 1893 cluster region ($r \le 10^{\prime}$, open circles) identified by Eswaraiah et al. (2011) on the basis of polarimetric and photometric observations.
 Using the theoretical isochrone of 4 Myr (Z = 0.02; log age = 6.6 yr) by Girardi et al. (2002) we estimated a distance of $3.3 \pm 0.4$ kpc which is in agreement with the distance (3.25 kpc) obtained by S07. Hence in the present study we use the distance to the cluster as $3.3 \pm 0.4$ kpc.

\section {Pre-main-sequence members in the region}
\begin{figure*}
\resizebox{12cm}{12cm}{\includegraphics{Fig2.eps}}
\caption{$V,(V-I)$ CMD for the YSOs identified by P11 in the NGC 1893 region.
The thick curve is the isochrone for 4 Myr from Girardi et al. (2002). Thin
curves are the PMS isochrones for 0.1, 1, 5 and 10 Myr by Siess et al. (2000).
The dashed curves represent evolutionary tracks for different masses by Siess
et al. (2000). All the isochrones and tracks are corrected for the distance
and reddening. The filled and open circles represnt Class II and Class III
sources respectively. The arrow shows the reddening vector.}
\label{fig2}
\end{figure*}

Fig. 2 shows $V/(V-I)$ CMD for the optical counterparts of the YSOs  (646 Class II and 425 Class III sources) identified by P11. In Fig. 2 we have also plotted post main sequence isochrones of 4 Myr with solar metallicity by Girardi et al. (2002) as well as pre-main-sequence isochrones by Siess et al. (2000). All the isochroes are adjusted for the cluster distance of 3.3 kpc and reddening $E(B-V)$ = 0.40 mag. Almost all the Class III sources have ages $\mathrel{\hbox{\rlap{\hbox{\lower4pt\hbox{$\sim$}}}\hbox{$<$}}}$ 5 Myr, whereas a significant number of Class II sources, as also pointed out by P11, are located below the 5 Myr PMS isochrone. P11 discussed that these could be candidate members with anomalous optical colours and/ or magnitude due to the disk related phenomena. In the case of W5 E {\mbox{H{\sc ii}~}} region ($l= 137\mbox{$^{\circ}$}.2$, $b= 0\mbox{$^{\circ}$}.92$) Chauhan et al. (2011) have found a significant amount of contamination in the sample of YSOs identified by Koenig et al. (2008) on the basis of {\it Spitzer} data. Chauhan et al. (2011) used $(J-H)/ (H-K)$  colour - colour diagram to avoid the contamination due to field star population in the YSO sample selected on the basis of {\it Spitzer} data.  Since NGC 1893 is located in the galactic plane, the cluster region is expected to be significantly contaminated by foreground as well as background stars (see S07). To understand the star formation scenario in the region, it is necessary to consider only those stars which are associated with NGC 1893 region. To avoid the contamination in the sample of YSOs given by P11 we adopted the following
approach.

\subsection {Identification of pre-main sequence stars}
Figs 3a (left panel) and 3b (right panel) display NIR colour - colour (NIR- CC) diagrams for the Class II and Class III sources identified by P11. In Fig. 3 the thin and thick dashed curves represent the unreddened main-sequence and giant branches (Bessell $\&$ Brett 1988), respectively. The dotted line indicates the locus of intrinsic CTTSs (Meyer et al. 1997). The curves are in the CIT system. The parallel dashed lines are the reddening vectors drawn from the tip of the giant branch (``upper reddening line''), from the base of the main-sequence (MS) branch (``middle reddening line'') and from the base of the tip of the intrinsic CTTSs line (``lower reddening line''). The extinction ratios $A_J/A_V = 0.265, A_H/A_V = 0.155$ and $A_K/A_V=0.090$ have been adopted from Cohen et al. (1981). The NIR-CC diagram is classified into three regions (cf. Ojha et al. 2004a,2004b). `F' region is located between the upper and middle reddening lines and the sources lying in this region could be either field stars (main-sequence stars, giants) or Class III and Class II sources with small NIR excesses. The `T' region is located between the middle and lower reddening lines.  The `T' region sources are considered to be mostly CTTSs (Class II objects). There may be an overlap in NIR colours of Herbig Ae/Be stars and CTTSs in the `T' region (Hillenbrand et al. 1992). The `P' region is redward of the `T' region and the sources lying in this region are  likely Class I objects (protostar-like objects; Ojha et al. 2004b). Therefore  objects falling in the `T' and `P'  regions of NIR-CC diagram could be probable Class II members associated with the cluster region. It is worthwhile, however, to mention that Robitaille et al. (2006) have recently shown that there is a significant overlap between protostars and CTTSs in the NIR-CC space.

\begin{figure*}
\resizebox{6cm}{6cm}{\includegraphics{Fig3a.eps}}
\resizebox{6cm}{6cm}{\includegraphics{Fig3b.eps}}
\caption{(a) NIR CC diagram for all the sources classified as Class II sources
in the catalogue by P11. The $JHK$ data for open circles have been taken from
2MASS catalogue. The thin and thick dashed curves represent the unreddened
main sequence and giant branches (Bessell $\&$ Brett 1988), respectively.
The dotted line indicates the locus of intrinsic CTTSs (Meyer et al. 1997).
The curves are also in the CIT system. Considering the errors in the data, we
consider only those sources as PMS sources associated with the region which
lie above the continuous line. The parallel dashed lines are the reddening
vectors drawn from the tip of the giant branch (``upper reddening line''), from the base of the main-sequence branch (``middle reddening line'') and from the
base of the tip of the intrinsic CTTS line (``lower reddening line''). (b) Same as Fig. 3a but for Class III sources.  }
\label{fig3}
\end{figure*}

Fig. 3a reveals that a large number of sources classified as Class II lie below the intrinsic locus of CTTSs. The sources having $(H-K) \mathrel{\hbox{\rlap{\hbox{\lower4pt\hbox{$\sim$}}}\hbox{$<$}}}$ 0.3 mag and lying below the extension of the intrinsic CTTSs locus could be reddened ($A_V \sim 2 -4$ mag) background MS stars. Fig. 3b also shows that a few Class III sources having $(J-H) \mathrel{\hbox{\rlap{\hbox{\lower4pt\hbox{$\sim$}}}\hbox{$<$}}}$ 0.5 mag are located around the unreddened MS locus. The location of these sources in $V/ (V-I)$ CMD also corresponds to the upper MS locus with magnitude brighter than $V\sim $15 mag (cf. Fig. 2). Damh \& Simon (2005)
have identified CTTSs and WTTSs in NGC 2264 region on the basis of the
H$\alpha$ sources. A comparison of NIR-CC diagrams for the Class II and Class III sources of NGC 1893 (Fig. 3) with the NIR-CC diagrams of CTTSs and WTTSs in the NGC 2264 region (cf. figure 16 by Dahm \& Simon 2005) manifests that the sample of YSOs identified by P11 is stongly contaminated by field populations. In Fig. 3 we plot a continuous line parallel to the intrinsic CTTS locus. Considering the errors in the data, we consider only those sources as PMS sources associated with the region which lie above the continuous line.  The above criteria yield 367 and 246 Class II and Class III sources, respectively with optical counterparts.

\section {AGE AND MASS ESTIMATION}

\begin{figure}
\centering
\resizebox{12cm}{12cm}{\includegraphics{Fig4.eps}}
\caption{ $V$ vs $V-I$  CMD of the selected YSOs. The isochrone for 4 Myr age (thick solid line) by Girardi et al. (2002) and PMS isochrones of 0.1, 1, 5 and 10 Myr (thin lines)  along with evolutionary tracks (dashed lines) of different mass stars by Siess et al. (2000) are also shown. All the isochrones are corrected for a distance of 3.3 kpc and reddening $E(B-V)=0.4$ mag. The symbols are same as in Fig. 2. }
\label{fig4}
\end{figure}

Fig. 4 shows $V/ (V-I)$ CMD for all the selected YSOs in the region as mentioned in Sec 4. In Fig. 4 we have also plotted the isochrone for 4 Myr by Girardi et al. (2002), which practically represents the zero-age-main-sequence (ZAMS), along with  the PMS isochrones for 0.1, 1, 5, 10 Myr with solar metallicity by Siess et al. (2000). The distance and  reddening $E(B-V)_{min}$ have been taken as 3.3 kpc and 0.4 mag (cf. Sec 3 and S07). Fig. 4 manifests that the contamination due to non-members is greatly reduced by applying the selection criterion as mentioned in Sec. 4. A similar case has been observed in W5 E region by Chauhan et al. (2011). The CMD (Fig. 4) shows a fairly well similarity with the statistically cleaned CMD as shown by S07 and also reveals an age spread in the cluster region.
Although the contamination is significantly reduced, still we can notice a few sources classified as Class II sources by P11 below the 5 Myr PMS isochrone. The CMD for TTSs identified on the basis of H$\alpha$ emission stars in the NGC 2264 region (Dahm \& Simon 2005) and in the IC 1396 region (Barentsen et al. 2011) shows a significant number of sources below 10 Myr isochrone. Barentsen et al. (2011) have discussed these sources and concluded that these could be background objects. To avoid the contamination due to background stars, we have considered only those sources as the PMS objects associated with NGC 1893 which are located above the 5 Myr isochrone.  This selection yields 298 and 240 Class II and Class III sources, respectively.

 The age and mass of each YSO, given in Table 1\footnote{The complete Table is available only in electronic form.}, are estimated by using the $V, (V-I)$ CMD, as discussed by Pandey at al. (2008) and Chauhan et al. (2009). Here we would like to point out that the estimation of the ages and masses of the PMS stars by comparing their locations in the CMDs with the theoretical isochrones is prone to random as well as systematic errors (see e.g. Hillenbrand 2005, Hillenbrand 2008, Chauhan et al. 2009, 2011). The effect of random errors due to photometric errors and reddening estimation in determination of ages and masses was estimated by propagating the random errors to their observed estimation by assuming normal error distribution and using the Monte-Carlo simulations (see e.g, Chauhan et al. 2009). The estimated ages and their errors are also given in Table 1.
The systematic errors could be due to the use of different PMS evolutionary models and the error in distance estimation etc. Since we are using evolutionary models by Siess et al. (2000) to estimate the age of all the YSOs in the region, we presume that the age estimation is affected only by the random errors.
The presence of binaries may be the another source of error in the age determination. Binarity will brighten the star, consequently the CMD will yield a lower age estimate. In the case of an equal mass binary we expect an error of $\sim$ 50 - 60\% in the PMS age estimation. However, it is difficult to estimate the influence of binaries/variables on mean age estimation as the fraction of binaries/variables is not known. In the  study of TTSs in the {\mbox{H{\sc ii}~}} region IC 1396, Barentson et al. (2011) presumed that the number of binaries in their sample of TTSs could be very low as close binary lose their disc significantly faster than single stars (cf. Bouwman et al. 2006).
Estimated ages and masses of the YSOs ranges from $\sim $ 0.1 to 5 Myr and $\sim $ 0.1 - 3.0 $M_\odot$ respectively, which are comparable with the lifetime and masses of TTSs.

\section {STAR FORMATION AND DISK EVOLUTION}
Massive O-type stars may have strong influence and significantly affect the entire star forming regions.  Energetic stellar winds from massive stars, on one hand, could evaporate nearby cloud and consequently terminate  star formation. Alternatively stellar winds and shock waves  may squeeze molecular cloud clumps and induce subsequent star formation. The morphological details of the environment and distribution of the YSOs in the NGC 1893 region can be used to probe the star formation scenario in the region. Here we felt worthwhile to compare the star formation scenario in the NGC 1893 region with that in the IC 1396 star forming region located at a distance of 870 pc and has rather similar morphology like NGC 1893.

\begin{figure*}
\resizebox{6cm}{6cm}{\includegraphics{Fig5a.eps}}
\resizebox{6cm}{6cm}{\includegraphics{Fig5b.eps}}
\caption{ False color composite image using the {\it Spitzer} observations (blue:3.6 $\mu$m, green:4.5 $\mu$m, red:8.0 $\mu$m) of NGC 1893 (left panel) and IC 1396 (right panel) regions. North is up, and East is to the left. }
\label{fig5}
\end{figure*}

\subsection {Morphology}

Figure 5 shows  colour composite images (blue: 3.6 $\mu$m, green: 4.5 $\mu$m, red: 8.0 $\mu$m) from {\it Spitzer} observations for NGC 1893 and IC 1396 regions. Both the regions, NGC 1893 and IC 1396, have globules  at a radial distance of $\sim$ 5.5 pc and  $\sim$ 4.5 pc respectively from the cluster centre. The ages of these clusters are $\mathrel{\hbox{\rlap{\hbox{\lower4pt\hbox{$\sim$}}}\hbox{$<$}}}$ 4 Myr and both clusters contain  massive O-type stars  at the center those regulates the star formation activity through stellar radiation and/ or wind (S07, Sicilia-Aguilar et al. 2005). Although NGC 1893 contains five O-type stars and 12 B1-type stars at various locations in the complex, the region is mainly powered by an O7.5 (HD 242935) star at the cluster center.
The IC 1396 region contains cluster Tr 37 with two O-type and 12 stars earlier than B1-type. The region is mainly powered by an O6 star (HD 206267) which is a member of the cluster Tr 37 and has several globules as well as BRCs at its periphery. In the case of IC 1396, it is believed that an expanding IF might have interacted with the molecular cloud and presently seen as globules and BRCs. NGC 1893 has a high density region on the south-west side and low density matter towards the north-east direction  which allows the matter to flow thus producing a typical "champagne flow" morphology (cf. Maheswar et al. 2007). The two pennant nebulae Sim 129 and Sim 130 are situated in the champagne flow direction.

Chen et al. (2004) and Sharma et al. (2006) have discussed that the initial stellar distribution in star clusters may be governed by the structure of parental molecular cloud as well as how star formation proceeds within the cloud. Later evolution of the cluster may be governed by internal gravitational interaction among member stars and external tidal forces due to the
Galactic disc or giant molecular clouds. S07 have studied the morphology of the cluster NGC 1893 on the basis of isodensity contours generated from optical ($V\le 18$) as well as from NIR 2MASS data. The isodensity contours indicate that the cluster NGC 1893 has elongated morphology. In Fig. 6 we have plotted the isodensity contours for the YSO sample identified in Section 4.1. The contours are plotted above  $1\sigma$ level. The distribution of YSOs indicates that the cluster NGC 1893 has elongated morphology which agrees well with the morphology obtained by S07. Since the cluster is not dynamically relaxed (S07), the present morphology of the cluster NGC 1893 may be governed by the star formation process.

\begin{figure*}
\resizebox{12cm}{12cm}{\includegraphics{Fig6.eps}}
\caption{ Isodensity contours for the YSOs identified in the present study. The contours are plotted above $1\sigma$ level. The contours have step size of 2 stars/ arc-min$^{2}$ with the lowest contour representing 4 stars/ arc-min$^{2}$. The maximum stellar density is 40 stars/ arc-min$^{2}$ . North is up and East is to the left. }
\label{fig6}
\end{figure*}

\subsection {Spatial distribution of YSOs}

\begin{figure*}
\resizebox{6.2cm}{6cm}{\includegraphics{Fig7a.eps}}
\resizebox{6.3cm}{6cm}{\includegraphics{Fig7b.eps}}
\caption{ Left Panel: The distribution of selected YSOs (Class II: filled  circle, Class III: open circles) in NGC 1893 region. The positions of the emission nebulae Sim 129 and Sim 130 are marked with large plus sign. The distribution of O-type stars with their spectral types is marked with small plus signs.
The sources bounded by the straight lines have  been used to study the age distribution of the YSOs (see right panel).  Right panel: The  age distribution of YSOs lying within the marked region (see left panel) as a function of radial distance from  the ionising source HD 242935 of NGC 1893 region.}
\label{fig7}
\end{figure*}

On the basis of distribution of H$\alpha$ emission and NIR excess stars S07 and Maheswar et al. (2007) have argued that star formation in the region have taken place through the RDI process. Fig. 7 (left panel) shows spatial distribution of all the selected YSOs in the NGC 1893 region as described in Sec 4.
Fig. 7 (left panel) reveals a rather aligned distribution of YSOs from the ionization source to the direction of nebulae as reported by Maheswar et al. (2007). Fig. 7 (right panel) displays the age distribution of YSOs lying within the region bounded by continuous lines in the left panel as a function of radial distance from the ionization source HD 242935, which manifests a scatter in the ages ($\sim$ 3-4 Myr) of YSOs lying in the  cluster region (r $\mathrel{\hbox{\rlap{\hbox{\lower4pt\hbox{$\sim$}}}\hbox{$<$}}}$ 5 arcmin), whereas  YSOs located near the nebulae at the periphery of the cluster have rather smaller ages in comparison to the YSOs lying in the cluster region. This further supports the notion of triggered star formation in the region due to RDI process as suggested by Maheswar et al. (2007) and S07. In the case of the Tr 37/ IC 1396 globule region Sicilia-Aguilar et al. (2004)
have shown that the H$\alpha$ emission stars (i.e., TTSs) are found to be aligned towards the direction of IC 1396 globule from the ionizing source, HD 206267 (O6 star). They also reported that most of the younger ($\sim$1 Myr) members appear to lie near or within the IC 1396 globule and concluded that it can be indicative of the triggered star formation. The age distribution of YSOs located between Tr 37 and IC 1396 globule as a function of radial distance from the star HD 206267 is shown in Fig. 8, which reveals a distribution rather similar to that shown in Fig. 7 (right panel). The ages of the YSOs have been taken from Sicilia-Aguilar et al. (2004). The ages of the YSOs located at $r \mathrel{\hbox{\rlap{\hbox{\lower4pt\hbox{$\sim$}}}\hbox{$>$}}}$ 12 arcmin have relatively
lower ages. A similar trend has recently been found for YSOs associated with the NGC 281 region (Sharma et al. 2012). In the case of a few BRCs Chauhan et al. (2009) have also reported that the  H$\alpha$ emission and NIR excess stars show an aligned distribution from the ionizing source to the direction of bright rims.

\begin{figure}
\centering
\resizebox{12cm}{12cm}{\includegraphics{Fig8.eps}}
\caption{Age distribution of YSOs towards the  direction of IC1396 globule as a function of radial distance from the O6.5 ionizing star HD 206267 of Tr37.}
\label{fig8}
\end{figure}

Figure 9 compares the radial distribution of YSOs in the NGC 1893/ Sim 129 \& 130  and Tr 37/ IC 1396 regions. The upper and lower insets in Fig. 9 display the fraction of CTTSs (assuming that all Class II sources and Class III sources are CTTSs and WTTSs respectively), $f_{CTTS} = (N_{CTTS}/ N_{CTTS}+N_{WTTS})$ towards the direction of the nebulae  and for the whole cluster  region respectively, as a function of projected radial distance from the ionization source. The fraction $f_{CTTS}$ shows an increasing trend as we move away from the ionization source. In the case of NGC 2244, Balog et al. (2007) have found that the fraction of stars with disk does not correlate with the distance, however they found a deficit of disks within the 0.5 pc radius from the O stars. Johnstone et al.(2004) have reported that the far-UV radiation from nearby massive star(s) may cause photoevaporation of YSO disks resulting in short ($\sim$ 10$^{6}$ yr) disk lifetimes. In the case of IC 1396 Barentsen et al. (2011) have concluded that the spatial gradient of IR excess is unlikely to be explained by photoevaporation alone. Roccatagliata et al. (2011) in the case of IC 1795 association do not find any systematic variation in the spatial distribution of disks within 0.6 pc of O-type star. The theoretical calculations predict that external UV radiation due to high-mass star can photoevaporate outer disks only within 0.3-0.7 pc (see e.g., Johnstone et al. 1998, Adams et al. 2004, Clarke 2007).

\begin{figure*}
\resizebox{6cm}{6cm}{\includegraphics{Fig9a.eps}}
\resizebox{6cm}{6cm}{\includegraphics{Fig9b.eps}}
\caption{Left panel: The distribution of Class III (open circles) and Class II (filled circles) YSOs in NGC 1893 region. The concentric annuli around the center have a width of 1\mbox{$^{\prime}$}. The solid line demarcates the sample of YSOs towards and opposite direction of the nebuale. The upper and lower insets show variation of $f_{CTTS}$ as a function of radial distance from the cluster center towards the direction of the nebulae and for the whole cluster region respectively.
Right panel:  Same as left panel but for Tr 37/ IC 1396 region.}
\label{fig9}
\end{figure*}

\subsection {Evolution of disk of TTSs}

As discussed in Sec 5, the YSOs selected in the present study have masses less than $\sim$ 3$\mbox{\rm $M_{\odot}$~}$, hence these YSOs are likely to  be TTSs. Recently, a considerable interest has been evolved to study the evolution of circumstellar disks around the YSOs (e.g., Haisch et al. 2001, Sicilia-Aguilar et al. 2006, Carpenter et al. 2006, Chauhan et al. 2009). The motivation to study the disk evolution lies in the fact that circumstellar disks are the potential sites of planet formation. In fact  the observed masses, sizes and chemical composition of young circumstellar disks are found to be analogous to that the protosolar nebula
(e.g., Beckwith 1999, Hillenbrand 2005). Characterization of the disk evolution can improve the understanding of the planet formation. Different observational diagnostics, such as emissions lines, UV excess, NIR/ MIR excess, millimeter and sub-millimeter excess are being used to study the temporal evolution of circumstellar disks. These diagnostics trace different properties of the disks at different scales, e.g., emission lines and UV excess trace level of accretion activity, IR excess traces the hot inner disk, whereas millimeter and sub-millimeter excess trace cold dust in the outer disk. Most of the disk evolution studies available in the literature are based on the NIR/ MIR excess which traces the evolution of inner accretion disks and it is found that in majority of the cases the inner disk does not last for more than $\sim$ 6 Myr (see e.g., Haish et al. 2001). However, there are a few open questions such as whether disk material dissipates at all radii simultaneously or inner disk disappears first and propagates outwards, whether the dissipation of disk depends on stellar masses and whether the CTTSs evolve to WTTSs.
Carpenter et al. (2006) have found that the evidence for mass  dependent circumstellar disk evolution, in the sense that the mechanism for disk dispersal operates less efficiently for low mass stars.

The ``standard model" by Kenyon \& Hartmann (1995) suggests that the CTTSs evolve to the WTTSs by losing the inner part of circumstellar disk. The age distribution of TTSs in the Taurus region indicates that the WTTSs are systematically older than the CTTSs, but the statistical significance was low (Kenyon \& Hartmann 1995; Hartmann 2001; Armitage et al. 2003). In the case of Taurus-Auriga T-association Bertout et al. (2007) concluded that the observed age distribution of CTTSs and WTTSs in the region can be explained by assuming that a CTTS evolves into a WTTS. Chauhan et al. (2009) have studied evolution of disks of TTSs associated with BRCs and supported the conclusion of Bertout et al. (2007) that CTTS evolves into a WTTS. On the other hand, there have also been many observations which claimed that the CTTS and the WTTS are coeval and have indistinguishable stellar properties (e.g., Walter et al. 1988; Lawson et al. 1996; Gras-Velazquez \& Ray 2005). From the analysis of the HR diagram of the CTTSs and WTTSs in Chamaeleon I, Lawson et al. (1996) concluded that some stars may be born even almost diskless or lose the disk at very early stages (age $<$ 1 Myr).  In such cases the coeval distribution of Class II sources (CTTSs) and Class III sources (WTTSs) does not invalidate the paradigm that CTTSs evolve to WTTSs.

\begin{figure}
\centering
\resizebox{12cm}{12cm}{\includegraphics{Fig10.eps}}
\caption{Left panel: Cumulative distributions of WTTSs of NGC 1893 region in two mass bins as a function of stellar age. Middle panel: Same as left panel but for CTTSs. Right Panel:  Cumulative distributions of CTTSs and WTTSs  in the mass range  0.2 $<$\mbox{\rm $M_{\odot}$~} $\le$ 1.0  as a function of stellar age}
\label{fig10}
\end{figure}

In the present work, we have estimated ages of 538 TTSs (see Sec. 5), hence the sample can be used to explore the answers to some of the above questions. In Fig. 10 we compare cumulative distribution of Class III (presuming as WTTSs; left panel) and Class II (presuming as CTTSs; middle panel) sources lying within the NGC 1893 cluster region and  having masses in the range 0.2 $<$ M/\mbox{\rm $M_{\odot}$~} $\le$ 0.4 and 0.4 $<$ M/\mbox{\rm $M_{\odot}$~} $\le$ 1.0, respectively. Fig. 10 (right panel) compares the cumulative distribution of Class II and and Class III sources having masses in the range of 0.2 $<$ M/\mbox{\rm $M_{\odot}$~} $\le$ 1.0. The cumulative age distributions of WTTSs and CTTSs in two mass bins (Fig. 10, left and middel panels respectively) indicates that the sources having masses $\sim 0.4 < M/M_\odot \le 1.0$ are relatively younger than WTTSs/ CTTSs having lower masses.  The Kolmogorov - Smirnov (KS) test confirms that the cumulative distributions of WTTSs and CTTSs in these two mass bins are different at a confidence levels of $\sim$ 80\% and $>99\%$ respectively.  This is a quantitative evidence supporting  the notion that the mechanisms for disk dispersal operates less efficiently for low-mass CTTSs. A similar result has been  derived on the  basis of disk fraction of TTSs in different mass bins by Carpenter et al. (2006) and references therein.
Roccatagliata et al. (2011) have found that the disk fraction in IC 1795 also depends on the stellar mass. They found that the  sources with masses $>2 \mbox{\rm $M_{\odot}$~}$ have a disk fraction of $\sim 20\%$, while lower mass objects ($\sim 0.8 < M/M_\odot \le 2.0$) have a disk fraction of $\sim 50\%$ which implies that disks around massive stars have a shorter dissipation timescale.

The cumulative distributions of WTTSs and CTTSs in the mass range 0.2 $<$ M/\mbox{\rm $M_{\odot}$~} $\le$ 1.0 reveal that these two distributions are different at a confidence level of $\sim 90\%$ suggesting that the WTTSs are younger in comparison to the CTTSs. This result is in contradiction with that recently found by Chauhan et al. (2009) in the case of CTTSs and WTTSs (classified on the basis of H$\alpha$ EW) associated with six BRCs and by Bertout et al. (2007) in the case of Taurus-Auriga T association. However, the above result is in agreement with those which claim that the CTTSs and WTTSs are coeval and have indistinguishable properties (e.g., Walter et al. 1988, Lawson et al. 1996, Gras-Velazquez \& Ray 2005, Chauhan et al. 2011).  P11 also has reported that the age and mass distribuions of Class II and Class III sources in the NGC 1893 are similar.

\subsubsection {Comparison with IC 1396}

\begin{figure}
\centering
\resizebox{12cm}{12cm}{\includegraphics{Fig11.eps}}
\caption{Cumulative distribution of CTTSs and WTTSs of Tr 37/ IC 1396 region in the mass range  0.3 $<$ M/\mbox{\rm $M_{\odot}$~} $\le$ 3.0 as a function of stellar age.
}
\label{fig11}
\end{figure}

Since the morphology and age of Tr 37/ IC 1396 is rather similar to that of NGC 1893, it will be worthwhile to compare the age distribution of CTTSs and WTTSs of NGC 1893 with those in the Tr 37/ IC 1396 globule region. The CTTSs and WTTSs in the Tr 37/ IC 1396 globule region are identified on the basis of EW of H$\alpha$ emission (stars having H$\alpha$ EW $\geq$ 10 {\AA}   are considered CTTSs). The data for EW and ages have been taken from Sicilia-Aguilar et al. (2005). Fig. 11 shows cumulative distributions of CTTSs and WTTSs of Tr 37 region having masses in the range $0.3 < M/M_\odot \le 3.0$  which indicates that although the distribution of WTTSs suggest higher ages for WTTSs, however the probability of these two samples belong to two different populations is only $\sim 30\%$.

\section{Summary}
On the basis of a comprehensive multi-wavelength study of the star forming region NGC 1893, we continued our attempt to understand the star formation scenario in and around the young cluster NGC 1893. The main results of the present work are enumerated as below:
\begin{enumerate}
\item The YSOs associated with the cluster region show an age spread of $\sim$ 5 Myr. The ages of the YSOs located near the nebulae at the periphery of the cluster have relatively smaller ages as compared to those located in the cluster region. The result is in accordance with our earlier result (S07, Maheswar et al. 2007) which support a triggered star formation towards the direction of the nebulae.

\item The density distribution of identified YSOs indicates an aligned distribution from the ionization source to the direction of the nebulae located at the periphery of the cluster. Since the cluster is not dynamically relaxed the alligned distribution of the YSOs may be an imprint of star formation process.

\item The fraction of disk bearing stars increases towards the periphery of the cluster.

\item There is an evidence supporting the notion that the mechanisms for disk dispersal operate less efficiently for low-mass stars.

\item The sample of Class II sources is found to be relatively older in comparison to that of Class III sources. This result is in contradiction with that recently found by Chauhan et al. (2009) in the case of CTTSs and WTTSs (classified on the basis of H$\alpha$ EW) associated with six BRCs and by Bertout et al. (2007) in the case of Taurus-Auriga T association. However, the above result is in agreement with those which claim that the CTTSs and WTTSs are coeval and have indistinguishable properties (e.g., Walter et al. 1988, Lawson et al. 1996, Gras-Velazquez \& Ray 2005).

\end{enumerate}

\section*{Acknowledgments}
The authors are thankful to the anonymous referee for useful comments. Part of the work was carried out by AKP during his visit to National Central University (Taiwan) under India-Taiwan collaborative program. AKP is thankful to the GITA, DST (India) and NSC (Taiwan) for the financial help. This publication makes use of the data products from the 2MASS, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology.

redpajama_set_name: RedPajamaArXiv


0843 NEWBOLD C.E. PRIMARY SCHOOL Halford, Idlicote Road, A429, Halford Bridge, A3400, Newbold on Stour, Moss Lane ( turn ), A3400, A429, Blackwell Road, Tredington, A3400, Newbold on Stour, Moss Lane.
1525 TREDINGTON C.E. PRIMARY SCHOOL Newbold, Moss Lane , A3400, A429, Blackwell Road, Tredington, A3400, A429, Halford, Idlicote Road, The Leys(turn), Idlicote Road, A429, unclassified road, A3400, Newbold.


text:
The United Kingdom has specific types of pedestrian crossing.

History

The first pedestrian crossing signal was erected in Bridge Street, Westminster, London, in December 1868. It was the idea of John Peake Knight, a railway engineer, who thought that it would provide a means to safely allow pedestrians to cross this busy thoroughfare. The signal consisted of a semaphore arm (manufactured by Saxby and Farmer, who were railway signaling makers), which was raised and lowered manually by a police constable who would rotate a handle on the side of the pole. The semaphore arms were augmented by gas illuminated lights at the top (green and red) to increase visibility of the signal at night. However, in January 1869, the gas used to illuminate the lights at the top leaked and caused an explosion, injuring the police operator. No further work was done on signalled pedestrian crossings until fifty years later.

In the early 20th century, car traffic increased dramatically. A reader of The Times wrote to the editor in 1911:"Could you do something to help the pedestrian to recover the old margin of safety on our common streets and roads? It is heartrending to read of the fearful deaths taking place. If a pedestrian now has even one hesitation or failure the chance of escape from a dreadful death is now much less than when all vehicles were much slower. There is, too, in the motor traffic an evident desire not to slow down before the last moment. It is surely a scandal that on the common ways there should be undue apprehension in the minds of the weakest users of them. While the streets and roads are for all, of necessity the pedestrians, and the feeblest of these, should receive the supreme consideration."

Types

Informal crossings

Pedestrian refuges are uncontrolled crossings with two dropped kerbs and a central traffic island, protected by kerbs. The island allows pedestrians to cross the road one direction of traffic at a time, which can be quicker and safer (they decrease pedestrian accidents by around 40%) than a lack of crossing. Additionally, they can narrow the road (refuges slow vehicle speeds by 6%) and prevent vehicles overtaking (as vehicles must normally pass the island on the left on a two-way road). However, they do not afford pedestrians priority, meaning pedestrians may have a longer wait than a controlled crossing. They can also create pinch points, which can be dangerous for cyclists.
Courtesy crossings are uncontrolled crossings with coloured surfacing or some other non-formal suggestion that pedestrians may cross. They aim to encourage concentrated pedestrian crossings and to encourage drivers to let pedestrians cross the roads out of courtesy, rather than obligation. The inclusion of stripes (e.g. in paving), the presence of narrowing and visual narrowings of the road positively affect courtesy.

Zebra crossings

Zebra crossings are a type of controlled crossing indicated by white longitudinal bars across the carriageway and upright flashing globes, known as 'belisha' beacons. Zebra crossings can be used on roads where the 85th percentile speed is not above 35mph. The minimum width for a crossing is 2.4 m.

At a zebra crossing, pedestrians should wait for traffic from both directions to stop before moving onto the crossing. Drivers are legally required give way when someone is crossing the road at a zebra crossing.

Signal-controlled crossings

Pelican crossings, puffin crossings and pedex crossings are all types of controlled crossing controlled by traffic signals for pedestrians and drivers. These types of crossings can be used where vehicle speeds are high, where there are a lot of vulnerable pedestrians, where vehicle flows or pedestrian flows are high or where the road layout could cause uncertainty.

At these crossings, there will be at least two signal heads facing each direction of vehicular traffic, as well as signal heads and call buttons for pedestrians. The crossings can be staggered to shorten crossing times, mainly for the benefit of vehicular traffic flow.

While pelican crossings are no longer permitted to be installed in Great Britain (they are in Northern Ireland), pedex crossings allow the continued use of farside pedestrian signals.

Defunct crossing types
Defunct crossings include:

 panda crossings

Pedestrian signals
There are two common types of pedestrian signal in the UK: nearside and farside. Nearside signals are incorporated into the push button, while farside signals are located at the other end of the crossing, facing the pedestrian across the road. Both types are permitted, and highway authorities can install either as they wish, though not both at the same installation.

Nearside signal units will normally be one unit, however a repeater unit may be provided higher up where there are lots of pedestrians, as nearside signals can be more easily blocked.

Farside signal heads will normally contain two signals: a red man and a green man signal. Furthermore, on the nearside there will be a push button unit, which normally contains the text "PEDESTRIANS push button and wait for signal opposite" as well as a pictorial guide to the crossing symbols.

Markings

Look right, look left

Road markings with the text "Look right" and "Look left" are sometimes used at pedestrian crossings to indicate to pedestrians the direction from which traffic will approach. Common uses may be a pedestrian island on a one way street or where a contraflow bus lane is in use. At times these markings have been painted incorrectly, which can create confusing situations for pedestrians. For example, on a street in Islington, the words "look right" were painted, although the accompanying arrow pointed left and traffic approached from the left.

Installation cost
Average installation costs are as follows. Note that the costs are based on no existing crossing, it will cost less in other cases (e.g. upgrading a puffin to a toucan).

The use of crossings by non-pedestrians

There are situations where other users may need to cross the road alongside pedestrians, in which case it may be practicable to use a multi-user crossing.

Parallel crossings are formed by placing a cycle track next to the bars in the zebra crossing, and allow cyclists to ride across the crossing, which they are not normally permitted to do. Toucan crossings are a type of controlled, signalised crossing which can be used simultaneously by pedestrians and cyclists, as cyclists cannot use the signal-controlled pedestrian crossings. Toucan crossings generally should not be staggered. Finally, a parallel crossing can be signalised by placing cycle track(s) in parallel to a puffin or pedex crossing. This is known as a sparrow crossing.

Equestrian crossings can be used by horse riders. They can be sited in parallel to toucan and pedestrian facilities.

For disabled pedestrians
All new and updated crossings in the UK, including informal crossings must not disable people. They do this is a number of different ways.

Dropped kerb: A ramp should be provided to assist pedestrians to cross the road, as some people, especially wheelchair users, find it difficult to negotiate kerbs. Therefore, a 'dropped kerb', where the kerb is flush with the carriageway, or a raised crossing is normally provided.

Tactile blister paving: Blister paving is always used at controlled and uncontrolled crossings. This is coloured red at controlled crossings (zebras, puffins, signalised junctions) and any other colour which contrasts from the footway surface at uncontrolled crossings.

The guidance recommends that pedestrian push buttons be located on the right side of the crossing waiting area. This is because visually impaired people are taught to look for a push button to their right.

References

Transport in the United Kingdom
Transport in Scotland
Transport in Wales
Transport in Northern Ireland
Transport in England
Pedestrian crossings

redpajama_set_name: RedPajamaWikipedia


text:
sidebar_content
Free Art Download: Testing a Bulletproof Vest, 1923
The things we'll do for a paycheck...
27 August,2013By Andrew Snavely
Free Art Downloads are easy and cheap to print. The white border is built in to simulate a matte, all you have to do is click the 'Download' button, then choose "File > Download" when the Google Drive window opens. Then, either print it yourself, or print it at a place like Staples or Costco for less than a buck. It's sized to fit an 11×14 frame, so it will need to be printed on 11×17 paper and trimmed along the included lines. The frame in the photo above is a $5 frame from the Wal-Mart photo department. For more detailed instructions, check out this article.
I love this photo. It's a strange thing to see, sure. But it's the subtext that gets me: Sometimes we do really crazy shit in the name of financial success.
Consider this fine fellow, W.H. Murphy, who is taking a .38 caliber bullet right to the chest, just to close a deal. On September 13, 1923, Murphy, who worked for the Protective Garment Corp. of New York, was in Washington, DC showing off his company's wares to the Fredrick County, Maryland Sheriff's Department.
Reportedly, Murphy didn't even blink when the bullet hit. Because he died instantly – kidding, kidding, Murphy was fine. The introduction of protective vests in the early 20th century was needed to combat the emerging criminal gangs utilizing their own homemade armor: several thick layers of cotton padding and cloth.
DIYFree Art DownloadFree StuffHome & Living
5 Job Hunting Techniques Your Peers Aren't Using
An Interactive Visual Guide to Whiskey
Primer's Visual Guide to Understanding Common Suit Features
Andrew Snavely 19 June,2012
Buying a suit isn't just deciding on a color. Learn the different options you'll be faced with and which to choose.
The Only 4 Reasons Why Your Peers Are More Successful than You
Jack Busch 16 January,2011
Do you know people who had the same grades as you but since leaving college have flown by you on the success train? Don't give up hope, Jack Busch has identified the only 4 reasons for early achievers... [more]
How to Serve Wine
Jack Busch 5 October,2011
Whether you're sharing some wine with friends over a home-cooked meal or celebrating with a bottle of champagne with your girlfriend's parents, getting the details right not only allows everyone to ... [more]

redpajama_set_name: RedPajamaCommonCrawl


text:
Home Top Stories Guv forwards death penalty petition for child rape to CMO
Guv forwards death penalty petition for child rape to CMO
Dimapur, April 16: Governor of Nagaland, PB Acharya has received a petition from chairperson cum national president of Confederation of Women Entrepreneurs of India, Uma Ghurka requesting to amend the law of Nagaland to award death penalty as punishment for child rape.
The Governor has extended supported to the petition and forwarded the same to the Chief Minister's Office for necessary legislation on the matter.
The letter, addressed to the Governor, said, "We need to play our role in the protection of the girl child," adding while there are many areas to tackle, the confederation believes an important aspect is severe punishment to the perpetrators.
It further stated that the Confederation of Women Entrepreneurs of India has initiated a petition asking for awarding death penalty or life imprisonment as punishment for child rape and speedy trial in case of child rape to get justice within six months.
The petition has received wide support from all sections of the society and over 15,000 people have signed in within a months' time and thousands of people continue to sign and propagate it every week. Also over 15 women organisations have extended their support to it, the letter stated.
Governor met Uma Ghurka in Mumbai and had talks with her regarding the matter. The Governor later asked Uma Ghurka to send a letter to his office.
Rajasthan, Madhya Pradesh, Haryana and Arunachal Pradesh have passed a bill awarding death penalty for rape of minor child below the age of 12.
Vice President calls for national movement against NCDs
Govt to impose penalty for misquoting Aadhaar
NAYO demands justice for Lt Neiphretuo
11 die in flood & landslides in Assam, 26.5 lakh people hit across 28 dists


text:
saint-paul luxembourg s. a. ist ein Luxemburger Verlagshaus in Form einer Aktiengesellschaft (société anonyme) mit Sitz in Luxemburg-Gasperich. Es geht auf die 1887 gegründete Sankt-Paulus-Gesellschaft zurück, die damals den Verlag und den Druck der 1848 geschaffenen katholischen Zeitung Luxemburger Wort, der größten Luxemburger Tageszeitung, übernahm. Ab 1915 firmierte das Unternehmen als Sankt-Paulus-Druckerei und als Imprimerie Saint-Paul, in Abkürzung ISP, um im Jahre 2000 den Namen saint-paul luxembourg anzunehmen, womit der erheblichen Ausweitung der Tätigkeitsfelder Rechnung getragen wurde. Zu diesem Zeitpunkt war das ursprünglich handwerklich geprägte Unternehmen unter die 20 größten Arbeitgeber des Landes aufgestiegen.

Obschon das Unternehmen bereits im 19. Jahrhundert nicht nur als Druckerei, sondern auch als Buchverlag tätig war, und es sich im 20. Jahrhundert ständig in weitere Geschäftsfelder hinein ausdehnte (wie das industrielle Drucken von Fremdprodukten, Buchbinderei, Buchhandel, Gestaltung von Werbung, audiovisuelle Produktion usw.), blieb jedoch, neben anderen Zeitungen und Zeitschriften im Verlag des Hauses, die populäre Qualitäts-Tageszeitung Luxemburger Wort jederzeit das weitaus wichtigste Produkt. Deswegen wurde und wird weiterhin, pars pro toto, das Unternehmen in seiner Gesamtheit im Luxemburger volkstümlichen Sprachgebrauch allgemein als d'Wort bezeichnet. Die Zeitung bleibt sowohl das beliebteste und einflussreichste Informationsmedium des Großherzogtums, als auch der wichtigste nationale Werbeträger. Deshalb hat ihre politische und philosophische Ausrichtung über viele Jahre hinweg in der Luxemburger Öffentlichkeit sehr polarisierend gewirkt.

Im 21. Jahrhundert hat saint-paul luxembourg seine Tätigkeiten weitgehend auf die Herstellung und den Vertrieb des Luxemburger Wort, in gedruckter wie elektronischer Form, sowie auf das Herausgeben einiger Wochenzeitungen eingeengt. Die französischsprachige Tageszeitung La Voix du Luxembourg und die Gratiszeitung Point 24 wurden eingestellt, nicht aber das populäre Wochenmagazin Télécran und die portugiesischsprachige Wochenzeitung contacto. Der Bogendruck und der Rotationsdruck im Heatset-Verfahren (Magazindruck) wurden aufgegeben, der Bücherverlag eingestellt, die Buchlädenkette geschlossen. Das Internet-Angebot der Zeitung ist viersprachig, um der kosmopolitischen Realität der Luxemburger Gesellschaft gerecht zu werden.

Bis zum Jahre 2020 gehörte das Unternehmen (direkt und indirekt) zu 100 % dem Erzbistum Luxemburg, wurde dann aber gänzlich an den internationalen Medienkonzern Mediahuis NV veräußert, der vor allem Tageszeitungen in Belgien, den Niederlanden und Irland herausgibt. Durch eine kleine Minderheitsbeteiligung seiner Vermögensverwaltungsgesellschaft Lafayette SA an Mediahuis bleibt das Erzbistum Luxemburg dem Verlag mittelbar verbunden.

Geschichte
Die Sankt-Paulus-Gesellschaft zur Verbreitung der katholischen Presse wurde durch notariellen Akt vom 20. November 1886 als anonyme Gesellschaft gegründet, und ihre Bildung wurde durch königlich-großherzoglichen Beschluss vom 9. Februar 1887 genehmigt. 86,9 % des Aktienkapitals gingen an den Drucker Johann Hary, der seinen Druckereibetrieb mit seinem gesamten Druckmaterial in die Firma einbrachte, und dessen Stiefsohn Louis Held, der das Amt des Bistumssekretärs bekleidete. Erster Direktor wurde der Geistliche Jean-Baptist Fallize, der jedoch bereits einige Wochen später vom Papst zum Apostolischen Administrator für Norwegen ernannt wurde. Später vererbte Louis Held die Aktienmehrheit an den Bischof von Luxemburg, weil das Bistum damals noch keine Rechtspersönlichkeit besaß.

Die Gesellschaft wurde hauptsächlich geschaffen, um die Herausgabe der seit 1848 bestehenden Zeitung Luxemburger Wort sicherzustellen, um deren Besitzverhältnisse es von 1879 bis 1884 heftige gerichtliche Auseinandersetzungen zwischen dem Redaktionskomitee und dem Drucker gegeben hatte. In ihren Anfängen war die Zeitung nacheinander bei verschiedenen Druckern hergestellt worden, ab Januar 1885 von der Sankt-Paulus-Druckerei des Herrn Hary.

Im April 2020 verkaufte das Erzbistum Luxemburg alle Anteile am Unternehmen an den belgischen Medienkonzern Mediahuis.

Literatur

 Pierre Gregoire: Das Luxemburger Wort für Wahrheit und Recht – Die Geschichte einer Zeitung in der Geschichte eines Volkes, Luxemburg 1936, 336 Seiten
 Pierre Gregoire: Hundert Jahre Luxemburger Wort, Luxemburg 1948, 140 Seiten
 Charles Jourdain: 100 Joër Sankt-Paulus-Dréckerei 1887–1987, Luxemburg 1987, 210 Seiten
 Gast Zangerlé: Bibliographie de l'Imprimerie Saint-Paul, Luxemburg 1988, 282 Seiten
 Georges Hellinghausen: 150 Jahre Luxemburger Wort – Selbstverständnis und Identität einer Zeitung 1973–1998, Luxemburg 1998; 470 Seiten, besonders (auf den Seiten 319 bis 375) das Kapitel VIII. Ausbau und Diversifizierung der ISP, sowie Teile der Anlagen
 150 Joër Wort – 150 Jahre und kein bißchen alt, Luxemburg 1998, 538 Seiten, besonders (auf den Seiten 283 bis 349) die Beiträge von Henri Leyder: Medienpol mit neun Satelliten – "Luxemburger Wort" und Sankt-Paulus-Druckerei, Paul Thill: 150 Jahre Bewegung im Zeitungsdruck, und Paul Zimmer: Die modernste Zeitungsdruckerei im weiten Umkreis
 saint-paul interna – Le journal du personnel du groupe saint-paul – Die Personalzeitung der ,saint-paul'-Gruppe, 1996–2002

Einzelnachweise

Weblinks
 Website

Medienunternehmen (Luxemburg)
Unternehmen (Luxemburg, Stadt)
Gasperich


text:
Energy Storage Program Opens Doors to Cleaner Air and More
Energy storage can dramatically improve the efficiency of the nation's existing fleet of fossil fuel-fired power plants, reduce emissions of greenhouse gas and help ensure a secure grid as more intermittent renewables (solar and wind power) are added to it, according to NETL Technology Manager Briggs White, Ph.D.
During a recent webinar held as part of ELECTRIC POWER Expo 2020, White outlined those and other benefits that the Advanced Energy Storage Program, established by the U.S. Department of Energy's (DOE) Office of Fossil Energy (FE), is expected the generate. White also highlighted NETL's development of data analytics, technologies for low-load operations and other advancements that have improved the efficiency of fossil assets.
White noted that NETL, which is managing the program for FE, has requested research organizations, universities and industry to provide proposals for funding in four main areas of energy storage technology (thermal, mechanical, chemical and hybrid). This supports the broader DOE-wide Energy Storage Grand Challenge, which was announced by U.S. Energy Secretary Dan Brouillette in January to position the United States as a world leader in energy storage by the end of the decade.
Visit electricpowerexpo.com to watch the recorded webinar featuring NETL's Briggs White.
The U.S. Department of Energy's National Energy Technology Laboratory develops and commercializes advanced technologies that provide reliable and affordable solutions to America's energy challenges. NETL's work supports DOE's mission to advance the national, economic and energy security of the United States.
NETL Drilling, Subsurface Research Featured in New Book
NCCC Achieves First Firing of Natural Gas Testing System, Demonstrating NETL Support for Carbon Capture Technology Research
NETL Researchers Publish Novel Geospatial Data Science Method in the Journal of Structural Geology for Predicting Faults and Fractures
NETL Leads ULTIMATE Project to Develop Ultrahigh-Temperature Alloys
Latest Edition of RWFI E-Note Monthly Released
Advancements in Rare Earth Elements Extraction Processes
DOE Invests Nearly $7.6 Million to Develop Energy Storage Projects
DOE Announces $4 Million for Projects to Optimize Safe, Secure, and Verifiable Carbon Storage
DOE Issues Request for Information to Attain Uninterruptable Supply of Critical Minerals
Myriad Successes for NETL's System Engineering and Analysis in 2020


Mothers Day is less than a month away and I thought, over the next few weeks, I'd share some simple ideas that every mom would appreciate (including me !) Almost every mom I know enjoys a hot cup of tea, specially in our desi culture! It's traditional to have tea and samosas when we have friends or relatives over. I'll be making a scented trivet which is perfect for such occasions. Your Mom will love this simple yet unique handmade gift.
Take your rice and put it in a ziplock bag . Add about 8/10 drops of your fragrance oil into the rice and close the bag. Mix the rice thoroughly and leave it overnight for the rice to infuse the oil.
The next day cut two nine inch squares from your fabric . With the wrong side facing up iron a quarter inch hem on one side of each square. Sew the three sides leaving the hemmed side open. Turn the fabric inside out. Make even lines across one side of the fabric. I made mine about one inch apart.
Sew on the marked lines making sure you keep your lines straight.
You will now have these small pockets to fill with rice.
You can use a funnel for this or make a paper cone to fill the pockets. I used a small milk jug with a spout that fit perfectly. Now let me warn you that filling the rice into these narrow pockets was not as easy as I thought . I found the best way to do this is to hold the bag straight up into the ziplock bag and start filling. This way the rice won't fall all over the place. Keep pushing the rice down so there are no air pockets . Remember to leave a one inch space at the end of each pocket.
Push the rice back and pin where the rice ends. Top stitch across to seal.
Even out the rice filling and you're done! Heat in the microwave for 60 seconds or until you reach the desired level of heat.Place your freshly made teapot on it and enjoy the aroma while sipping your tea.
You can use this as a trivet for your hot pans too, but you don't need to microwave it as the heat from the pan will release the fragrance from the rice.


7. Switch the ignition to ON.
8. Verify that voltage is B+ at the antenna amplifier terminal A.
If the battery voltage can be verified, replace the antenna amplifier.
If not as indicated in the table, replace antenna amplifier.


The Archipelago Los Roques National Park, off the coast of Venezuela is one of the most beautiful collection of beaches you can experience. Los Roques is located roughly 155 kilometers north of Venezuela's central coast, and about 80 miles (128km) north of the port of La Guaira, Venezuela's primary port.
One of the interesting things about Los Roques, Venezuela is that it's not just one piece of land. Los Roques is actually made up of approximately 350 islands, cays, and inlets that cover over 546 acres (221,120 hectares!), which makes the Los Roques National Park the biggest marine park in the Caribbean.
In 1589, the governor of the Venezuelan province ordered the take over of the Los Roques Achipelago on behalf of the Colony, despite protests by the Dutch who considered Los Roques to be a territory that belonged to them.
In the middle of the 20th century, Venezuelan fisherman began to inhabit Los Roques permanently, establishing a small town on Gran Roque Island, which still produces over 90% of the lobster people eat in Venezuela.
Then, in 1972 the Venezuelan government declared the Archipelago Los Roques a National Park to protect the large variety of seabirds, fish, coral reefs, and other marine life found all around the islands of Los Roques, Venezuela.
Why Travel to Los Roques, Venezuela?
Travelers flock to Los Roques from all over the world for it's beauty, the amazing diversity of marine life, the friendly hospitality, and all the fun outdoor activities you can experience in Los Roques, Venezuela. Because it is a regulated National Park, it is preserved from pollution, speculation and mass tourism. No massive real estate programs, with swimming pools and night clubs, no jet skis, no marinas, no microlight aircrafts … Los Roques is natural and authentic !
The shores surrounding the 350+ islands, cays and inlets that make up Los Roques, Venezuela are among the most beautiful beaches you will ever visit. The crystal clear, white sand beaches stretch as far as the eyes can see, and the water color changes dramatic shades as you look out deeper into the ocean.
or explore one of Los Roques National Park's many coral reefs on a scuba diving expedition with a certified scuba instructor.
The weather in Los Roques is one of the primary reasons so many people travel there year round. The air temperatures fluctuate from the 80s to low 90s (26º to 32 Celsius) Fahrenheit, which is a welcome relief to people visiting from colder areas of the world.
The water temperature off the coast of Los Roques stay about 76º Fahrenheit (about 24º Celcius) year round. Combine that with the trade-winds that provide a nice breeze throughout the day, and you have a perfect location to enjoy Bonefishing, deep sea fishing, kit surfing, or just relaxing on the sand as you admire this island paradise.
Most people find that the best way to travel to Los Roques National Park is a flight on Los Roques Airlines, from Caracas, Venezuela. It's a super short flight that will take you to Los Roques in just 35 minutes. And prices for flights to Los Roques National Park are reasonable, ranging from 0 – 0 per person for a round trip ticket, depending on the season.
The rooms at the various hotels (Posadas) in Los Roques are usually simple in layout, with a focus on comfort. Hotel rooms are clean, cozy, and have many of the creature comforts you'd want (including DirecTV satellite service), while on vacation on a beautiful Caribbean island. As you can imagine, the hotels rooms in Los Roques vary based on the size of the room, location, and extras included at the Hotel where you'll stay… but you can expect to find reasonable hotels ranging from – 0 per night throughout the islands, depending on the season. Some hotels in Los Roques even offer rental equipment and schools for Bonefishing, kite surfing, scuba diving, and many other fun outdoor activities.


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Home News Yemen And Masdar Signs Agreement To Build 120 MW Solar Power Plant...
Yemen And Masdar Signs Agreement To Build 120 MW Solar Power Plant In Aden
A file photo of Yemen And Masdar Signs Agreement To Build 120 MW Solar Power Plant In Aden
The UAE capital, Abu Dhabi, witnessed the signing of a joint cooperation agreement between the Ministry of Electricity and Energy in Yemen, and the Abu Dhabi Future Energy Company, Masdar, to provide the interim capital, Aden, with a solar power plant with a total capacity of 120 megawatts.
The agreement was signed on the Yemeni side by the Minister of Electricity, Engineer Manea bin Yameen, and the local authority in the interim capital, Aden, represented by the Minister of State, Governor of the capital, Ahmed Hamid Lamlas, and on the Emirati side, Eng. The future is Masdar.
The agreement provides for the establishment of a solar power plant with a capacity of 120 megawatts per hour. The agreement also includes the construction of transmission lines and transformer stations for the transmission and distribution of the energy that will be generated by the station, in addition to a number of items related to the conditions and obligations between the two parties.
Also Read OXAGON Signs Landmark MoU With Ministry Of Industry And Mineral Resources And MODON To Support Future Factories Program
The energy in Yemen will reduce the cost of generating electricity during daylight hours, as well as the need for fuel for power plants, and will also contribute to preserving the environment by reducing carbon emissions.
After signing the agreement, Eng. Bin Yammine confirmed that the survey work for the station had actually started a month ago, noting that there are tireless efforts being made to complete the project as soon as possible.
For his part, Lamlas stressed the strategic importance of the project, praising the unlimited support provided by the brothers in the UAE to rehabilitate the infrastructure in the interim capital, Aden.
Also Read Masdar Signs Agreement to Develop 1 GW of Renewable Energy Projects in Kyrgyzstan
Masdar
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We're two, going on three, years deep into the basket bag trend that just won't quit. From oversized beach totes and itty-bitty woven baskets starting things off, handbag designers everywhere have adopted straw, wicker, rattan, and even bamboo into their collections. And every season thus far, without fail, we've immediately begun adding them to our wish lists (just take our word for it, since our senior fashion market editor's collection has broken double digits). Luckily for us and our perilous spending habits, the trend is still growing stronger. Just thank Jane Birkin.


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Medly Pharmacy, EmblemHealth, The Campaign Against Hunger, and City Officials Join Forces to Give Away Turkeys to One Thousand Local Residents
BROOKLYN, N.Y., Nov. 19, 2020 /PRNewswire/ — Medly Pharmacy, a full-service, digital pharmacy that offers free same-day prescription delivery, announced today a joint food giveaway and flu vaccination event in partnership with EmblemHealth, one of the nation's largest not-for-profit health insurers. The event aims to reach vulnerable New Yorkers to ensure they have a safe and healthy Thanksgiving holiday. Medly Pharmacy and EmblemHealth are launching this initiative alongside The Campaign Against Hunger (TCAH) — an organization tackling food insecurity in New York. Eric Adams, the Brooklyn Borough President, will also be in attendance alongside Council Member Robert Cornegy Jr., State Senator Roxanne Persaud, Assemblymember Latrice Walker, Assemblymember Tremaine Wright, State Senator Zellnor Myrie, State Senator Kevin Parker, and Assemblymember Diana Richardson.
The initiative will take place in the Bedford-Stuyvesant neighborhood of Brooklyn. TCAH will give away turkeys and other traditional holiday foods to more than 1,000 residents in need, handing out nutritious holiday bags of food to all who have pre-registered ahead of the Thanksgiving holiday. Those who didn't get the chance to pre-register, may visit the TCAH food pantry free of charge, where they serve 14,000 families per week through sponsorships and donations. The opportunity to receive a flu vaccine will also be offered through Medly and EmblemHealth.
As flu season nears its peak, Medly and EmblemHealth believe that tackling the disparities in accessing vaccinations needs to be addressed more than ever. As colder weather exacerbates the spread of viruses and families come together for the holidays, the threat of illness is a serious concern. Medly and EmblemHealth believe that preventive health and nutritious food go hand in hand to ensure local communities have a safe Thanksgiving holiday. After two successful flu vaccination events targeting underserved populations in Brooklyn, and now with this third initiative, the partners are working to improve equitable access to care in their local communities.
Food insecurity rates have been soaring across the country due to the COVID-19 pandemic, exacerbating child hunger and disproportionately affecting communities of color. Brooklyn, which has historically had the highest levels of food insecurity of the five boroughs, was hit especially hard by the pandemic and continues to feel the ramifications — especially with recent COVID-19 spikes in New York.
"This initiative will make a tangible difference for many New Yorkers who haven't had access to a flu vaccine or know how they were going to put food on the table this Thanksgiving," said Dr. Marg Patel, CEO and Cofounder of Medly. "Proper nutrition and preventative health are complementary, and necessary, as we continue to fight the ramifications of the COVID-19 pandemic. I'm eager to stand side by side today with New York Elected Officials, The Campaign Against Hunger, and EmblemHealth as we commit to equitable access to food and care throughout our local communities."
"Whether it's a warm meal or a trusted local pharmacist who speaks their language, the resources people have access to have a long-lasting impact on their health and the health of their communities," said George Hulse, EmblemHealth Vice President and Senior Advisor to the CEO. "Many of the communities who have been disproportionately affected by COVID-19 are also struggling with food insecurity. I am proud to be a part of an initiative that tackles two issues in which these consequences are often, unfortunately, intertwined."
"Kids and families are going hungry in Brooklyn neighborhoods and across the city," said Dr. Melony Samuels, Executive Director and Founder of The Campaign Against Hunger. "Before the pandemic, 14.7% of Brooklyn residents were food insecure, which has only been on the rise since the onset of the pandemic. If you don't even know where you're going to get your next meal, then the barriers to healthcare are only amplified. I'm eager to get to work alongside Medly, EmblemHealth, and local elected officials to reach our most disadvantaged citizens and tackle the greatest needs along the full spectrum of health."
"In these challenging times, I am especially thankful for community partners," said New York City Councilman Robert Cornegy Jr. "The Campaign Against Hunger has been providing food with dignity to New Yorkers since 1998. Thanksgiving will look different from years past but love in our community is as strong as ever, especially with allies like The Campaign Against Hunger."
More information about the event is as follow:
Location: The headquarters for the Campaign Against Hunger: 2010 Fulton Street, Brooklyn, NY 11233.
Date: Thursday, November 19, from 10 AM EST to 3 PM EST
Additional donations: Additional donations can be made through the TCAH website: [https://bscah.secure.nonprofitsoapbox.com/donation](https://bscah.secure.nonprofitsoapbox.com/donation).
Vaccine details: Medly pharmacists will be on-site administering the vaccination, and available for any questions associated with the virus. Participants will receive the vaccination either free or at low cost based on their insurance plans. For more information and event details, please visit [www.medlypharmacy.com/flushot](https://www.medlypharmacy.com/flushot).
About Medly Pharmacy Medly Pharmacy is a full-service, digital pharmacy that delivers a patient's prescriptions to their door for free on the same day in New York City, New Jersey, Philadelphia, and Baltimore. The digital experience makes managing prescriptions simple, efficient, smart and most importantly, safe for customers. More information can be found at www.medlypharmacy.com.
About EmblemHealth EmblemHealth is one of the nation's largest nonprofit health insurers, with 3.2 million members and an 80-year legacy of serving New York's communities. The company offers a full range of commercial and government-sponsored health plans to employers, individuals and families, as well as convenient community resources. As a market leader in value-based care, EmblemHealth partners with top doctors and hospitals to deliver quality, affordable care. For more information, visit emblemhealth.com.
Media Contact: Baxter Townsend Baxter@Tuskstrategies.com (631) 697-8530


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Endorsements tennis 2 cristiano ronaldo $105 million
Brooklyn Nets HP Field House 2 PM • Memphis Grizzlies vs.
A: It's kind of weird because he has a Jets tattoo, so even if he wears a Saquon Barkley jersey, he's still repping the Jets.
Under Armour agreed to a 15-year contract with UCLA in 2016 that was the richest shoe and apparel sponsorship in college sports history, replacing adidas.
Downtown Flagstaff What's your Hidden Talent?
Carson Wentz $59 million $55 million $4 million NFL Upcoming Super Bowl Games • Super Bowl LV Raymond James Stadium Tampa Feb.
The NFL's changing international scenario comes as the league is monitoring its decision to move the annual Pro Bowl.
• Epix, a joint venture among Viacom Inc., its Paramount Pictures unit, Lionsgate and Metro-Goldwyn-Mayer Studios, had numerous solid hits in 2014 with in-depth and hard-hitting stories about the likes of Dwight Howard, David Ortiz, Oscar de la Hoya, Bethany Hamilton, the Forgotten Four and the NHL, among others.
Bumgarner is perhaps not the same caliber of pitcher at this stage of his career as Cole and Strasburg, nor is he the de facto ace he was when leading the Giants to World Series titles years ago.
Portland Trail Blazers The Arena, Orlando NBA TV 4 PM • Phoenix Suns vs.
Over 14 players competed at professional level last year which is simply too many.
Call to schedule.
If you would like to search for all players born on a certain day, for example all players born on December 25th in any year, choose the month and day with the drop down boxes and then choose the 'Month and Day Search' option.
Regarding the NHL Seattle Ice Centre, If we are awarded an NHL franchise, creating a one-of-a-kind training facility that can serve as the home of hockey in the Pacific Northwest for youth and adult hockey, all within the city of Seattle, is critical, Leiweke, CEO for NHL Seattle, said via the ownership group.
I start watching college on Jan.
Jackson's injury lingers, with no clear answer for the future.
On James Augustine?s pre-draft workouts:?He?s already worked out for a bunch of teams, and he?s scheduled to work out for a bunch more.
The technology will be used during MLB All-Star Week for events in Nationals Park in Washington DC, where a dedicated entrance near the third base side of the stadium will allow Clear members to enter.
New and expanded relationships with western sports organizations include Calgary Stampede, Days of '47 Cowboy Games & Rodeo, Cheyenne Frontier Days, WCRA , National High School Rodeo and Indian National Finals Rodeo.
How did you do it?
Memphis Grizzles Visa Athletic Center, Orlando 4 PM • Sacramento Kings vs.
The 2012 NCAA men's hoops tournament begins March 11 with Selection Sunday, custom uniforms which the participating schools will be named and placed into regions.
Brown tries to buy insurance from the Geico Gecko, or Mike Tyson returns a piece of the ear he bit off of Evander Holyfield to the former boxer, or Godzilla goes waterskiing and hangs out on the beach with other dudes, it may sound like the work of mad men or Lewis Carroll, but it's really part of the modus operandi at ad agency BBDO New York.
For us, for years we've played lots of three-deep .
For the 2018 survey, 50 consumers, 16 years of age from the nine U.S.
Neymar $95 million $79 million $25 million Soccer 5.
Los Angeles Clippers HP Field House, Orlando, ESPN 6 PM • Philadelphia 76ers vs.
New Orleans Pelicans HP Field House, Orlando TNT 6 PM • LA Clippers vs.
He claims that he's been around for a lot longer than we know https://www.amazon.com/dp/B086KZ2ZL1 and recent construction at the Wells Fargo Center disturbed his secret hideout forcing him to show his face publicly for the first time.
That was pretty amazing.
In an e-mail to UCLA constituents, athletic director Dan Guerrero wrote We are exploring all of our options to resist Under Armour's actions.
We use that information to verify your identity and to respond to your correspondence.
They also have Tennessee, Tampa Bay, the Los Angeles Chargers and Oakland Raiders on their upcoming schedule.


ACR 2018 Hill Day was the perfect way to punctuate an incredibly successful meeting. Hundreds of residents and fellows traveled to Washington, D.C., for a dizzying five days of programming, including hearing from the smartest and most fearless minds in radiology, querying expert panels, electing brand new leadership, and reuniting with old friends and meeting countless others. The meeting culminated with us joining our respective state caucuses, donning our most persuasive business attire, and heading to Capitol Hill.
More than 450 ACR members, including attendings, residents and fellows, and even a smattering of medical students, met with over 275 congressional offices to advocate on behalf of their patients. This year, our priority was to ensure that our patients had access to the full array of colon cancer screening options given the highest grade by the U.S. Preventive Services Task Force, including CT colonography. While CT colonography is required by the Affordable Care Act to be covered by most third-party plans, it isn't covered by Medicare — limiting access to this exam for patients 65 and over. As only three in five eligible adults in the United States are screened appropriately for colon cancer, we argued that our patients deserve access to whichever screening modality is right for them.
A second focus of our advocacy efforts was the Medicare Access to Radiology Care Act (MARCA). MARCA establishes the role of the radiology assistant (RA), to help perform diagnostic services under the direct supervision of a radiologist (as opposed to personal supervision, the current standard, which requires the radiologist to be in the room). With the ever-increasing demand for imaging services, RAs can play a critical role in enhancing a radiology department or practice's overall efficiency and improving access to care.
While there was lively discussion during the Council meetings regarding the RA's scope of practice, many concerns were alleviated by the assurances provided by stakeholders from the American Society of Radiologic Technologists and others that the role of the RA is both clearly defined and mutually understood, and includes an absolute ban on interpreting images. In the end, this issue served as a hopeful reminder of how the ACR operates. After an impassioned, candid, and thorough conversation, all ACR members provided a unified front as they met with their legislators in the name of improving access to patient care.
Now back home in Los Angeles, I can't help but reflect on that feeling of being in the thick of the action, working together with my fellow ACR members to make sure that the future radiology practice we envision is the one that prevails. I encourage anyone who wasn't able to make it this year to do what you can to get more involved with the College's advocacy efforts. Reach out to your state chapter, engage on Twitter, join a RFS subcommittee, join the Radiology Advocacy Network (email me for more information), or all of the above. Let's keep the momentum going until next year!


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The Red Solstice (PC) beginner's guide
Combat uniforms
Tactics mode
Auto-Aim
Mission Objectives
Opponent's choice
Fast level up
Combat uniforms / Class Overview
In The Red Solstice, first you have to select a combat suit and there are eight different classes. In multiplayer mode each player can take on another role, thus supporting the team. What advantages and disadvantages each class has, check out the following table.
Great Role Arms Special feature
Assault All-rounder Machine guns, grenade launchers, shotgun, pistol, SMG, Minigun The Assault is the class which alone can survive the longest. In connection with supporters, as the Medic, it becomes a fighting machine.
Medic Healer Light weapons, assault rifle, SMG The healer is effective only in the team. He can cure bleeding, poisoning and other injuries. But he must also be protected by his colleagues.
Demolition Damage Explosives, assault rifles The Demolition may employ various explosives to eliminate groups of enemies. Later, it can support the group with established turrets.
Recon Information / support Assault Rifle With its capabilities of Recon opponents feel lighter on and returns the position of key goals to his Group.
Heavy Support Damage Force Gun, Flamethrower, Minigun, Assault Rifle The Heavy cares about the damage to your enemies. For him there are numerous skills available that shorten its reload time and increase damage values.
Hell-fire Tank Flamethrowers, explosive projectiles, Minigun The Hellfire assumes the role of the tank. He stands in the forefront and takes opponents with his strong short-ranged weapons targeted.
Terminator Tank Energy weapons, minigun, explosive rounds Even the Terminator is a tank class. He uses more weapons with splash damage and can teleport later from sticky situations.
Marksman Damage Sniper rifles, assault rifle The Marksman is the sniper in the game. He stands in the back row and exerts targeted damage to important and dangerous goals for the group.
To survive in The Red Solstice, you must always be able to master. Here you can activate the Space bar to help in the tactic mode. This is slowed you enormously and you have time to organize your squad. This is particularly important in the story mode and in the wave attacks because there you take control over an entire team.
Have you slowed down the game, you can now give each team member individually commands. So spread your own: Marine strategically in the room, take cover behind square or bottlenecks Clearly mark with booby traps. So use the tactic mode as often as possible. So you can keep track and will rarely overwhelmed by your enemies.
During your adventures on Mars, you will arrive in ammunitions repeatedly. There is but one remedy. Search for various containers, give them the supplies for you. These include for example the supply crates that are spread all over the roads. Shoot them, there is a chance that they leave items such as magazines, explosives or medikits.
One step further is what the lockers inside buildings. These are divided into different degrees of success. Do you find a locker with higher quality, and the potential items are better or you get more of it. So keep permanent lookout for such containers to replenish your supplies.
To stand against the hordes of enemies in The Red Solstice, you don't have to click on each individual, there are the so-called Auto-Aim. Once you activate this the character will automatically take on the next best near target. This will save an enormous amount of ammunition. Because the Auto-Aim mode is much more accurate than manual shooting. By flares and skills you can improve it, but never compensated.
So use the Auto-Aim, if you have to overcome long distances or defending a position. So do it go onrushing opponents without having to stop. And in defending your team members can hold a position while their important mission objectives done in protection of their fire.
Since you always run in enemy hordes, you constantly have to check your ammunition. Once you have a short break, switch to the tactic mode. There you can watch in peace and reload the magazines of your weapons
Once you come across the game's addition tutorial, mission objectives will no longer appear to you directly. You gotta look at the map routes and escape routes that your network operator can call Escape. Respect always ensures that you have several options to find the route to a destination. Are nests or fall on the main path should choose alternative routes. These usually are fewer opponents.
Opponent's election
Are you on the way to a mission objective, you are constantly pursuing opponents. But most enemies cannot reach, because they move more slowly. So then turns off the Auto-Aim mode and take only opponent on the grain, which moves much faster than your group. So save your ammo and can use this later against powerful monsters and other abominations.
In almost all environments of The Red Solstice, there are numerous coverages, such as tables, fences and boxes. These objects can your fighter away shooting, opponents but not directly to you. Addiction therefore always covers options, so that you minimize incoming damage and maximize the damage to you.
Quick level up
As you keep track of your level, we tell you on this page.
While the missions in The Red Solstice constantly level up. Completed for each opponents, mission objectives or open containers get your fighters XP. Use the tactic to view repeatedly their skills. There you can improve and better prepare for the upcoming battles.
Red Solstice: gain
The so-called Reinforcements will occur more frequently as part of your mission. These landing sites in the game world must defend over a period of time until a flying ship settles your gain. Thus, players who have already left, put back into play and can move with you. However, this gain comes only if you have completed all the monsters in the landing zone. For this requires enormous firepower and numerous booby traps.
Especially towards the end of the countdown storm particularly strong copies an on you. Positioned behind you coverage possibilities and move here after you tried it with different characters. This you get less damage, and the remaining team members can fire undisturbed.
Explosives, such as mines, Claymores, or underground explosions are very strong items that can turn off multiple enemies with one. You've got to move in confined spaces and then usually manually ignited with the selected character. Waits for an entire group of enemies in the blast radius is displayed in order to maximize the damage.
But the explosives also caution. Ignite while team members are near, they also get injured. An incorrectly ignited charge can cost a player you already.
This is very dangerous especially in tricky situations with many enemies. Therefore, keep yourselves distance always and other explosive devices.
categories: The Red Solstice; PC; Beginner's Guide


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