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

\begin{figure}
\centering
\includegraphics[angle=0,width=0.4\textwidth]{intro.eps}
 \caption{\small{Overview of Sh2-205 region: the areas discussed in the paper are schematically indicated in the VTSS continuun image.}}
 \end{figure}

Observational studies have shown that expanding \hii regions and interstellar bubbles are surrounded by massive and dense slowly expanding shells. Stellar formation may be favoured within these dense envelopes around
\hii regions (Deharveng, Zavagno \& Caplan 2005) and stellar wind bubbles through the {\it collect
and collapse} mechanism first described by Elmegreen \& Lada (1977), which was analytically developed by Whitworth \etal (1994). Numerical simulations were performed by Dale, Bonnell \& Whitworth (2007). In \hii regions, this process can be summarized as follows: The supersonic expansion of an \hii region on their surroundings creates compressed layers where gas and dust are piled up between the ionization and the shock fronts. This shocked material grows in mass and may become gravitationally unstable. Under these conditions, the dense envelopes may break up forming massive cores which could become in nurseries for new generations of massive stars. Thus, the dynamical evolution of \hii regions provides the conditions for the star formation process to develop (Deharveng \etal2003, Zavagno \etal2006).

A similar process may act in the dense envelopes around interstellar bubbles. Indeed, young stellar object (YSO) candidates  have been found projected onto the neutral shells associated with some wind bubbles (e.g. Cappa \etal2005).

In a previous paper, we studied the ISM in the environs of Sh2-205, located at a distance of $\sim$ 1.0 kpc (Romero \& Cappa~2008, hereinafter referred to as Paper I). In that work, we showed the presence of three independent optical nebulae: \hbox{SH\,149.25--0.00}, \hbox{SH\,148.83--0.67}, \hbox{LBN\,148.11--0.45}, and an H\,{\sc i}~shell centered at \hbox{{\it (l,b)} = (149\degr 0\arcmin, --1\degr 30\arcmin)}.
For the sake of clarity, the areas discussed in the paper are indicated in Fig. 1. We determined that SH\,148.83--0.67 is an interstellar bubble powered by the stellar winds of HD\,24431. The origin of SH\,149.25--0.00, which can hardly be distinguished by its optical and faint radio emissions, remains an open question since no stellar object was found associated with the nebula. The shell centered at \hbox{{\it (l,b)} = (149\degr 0\arcmin, --1\degr 30\arcmin)}, of $\approx$ 2\fdg2 $\times$ 1\fdg5 in size, is placed at a kinematical distance of 1.5 kpc and may be related to the open cluster NGC\,1444.

The most striking area is LBN\,148.11--0.45. This is a classical \hii region of 30\arcmin $\times$ 24\arcmin~in size and \hbox{4 $\times$ 10$^{6}$ yr} in age. Neutral atomic and molecular gas in the velocity range \hbox{[--0.65, --11.1]} km\,s$^{-1}$~partially encircles this ionized region. It is also closely surrounded by a dust ring detected in the mid- and far-infrared, suggesting the presence of a PDR (photodissociation region) at the interface between the ionized and molecular regions. The derived ambient density (n$_{o}$ $\approx$ 800 cm$^{-3}$) indicates that this \hii region is evolving in a dense interstellar medium (Paper I).

The morphology of this \hii region encouraged us to look for signposts of stellar formation activity at its periphery. In this paper we investigate the stellar formation activity in the three different structures of Sh2-205 and in the large H\,{\sc i}~shell, based on infrared point source catalogues.

We organized the present paper as follows: Sect. 2 gives a brief description of the methods we used to find tracers of stellar formation activity; Sect. 3 shows the main results obtained for the four analyzed regions: \hbox{LBN\,148.11--0.45}, \hbox{SH\,148.83--0.67}, \hbox{SH\,149.25--0.00}, and the H\,{\sc i}~shell. Whether our findings are compatible with the collect and collapse process is discussed in Sect. 4. A summary of the main results is presented in Sect. 5.

\section{Datasets and Selection criteria}

\begin{figure*}
\centering
\includegraphics[angle=0,width=\textwidth]{ccd-cmd.eps}
\caption{\small{CC and CM diagrams of the 2MASS sources towards Sh2-205 and the control area. YSO and main sequence star candidates are indicated by triangles and squares, respectively. {\it Upper panels}: $(H-Ks, J-H)$ diagram of Sh2-205 (left panel) and a control field (right panel). The locations of the derredened early-type main sequence and giant stars are shown. The reddening curves for MO III stars (upper line) and O6-8 V stars (lower line) are indicated. {\it Lower panel}:  $(Ks, H-Ks)$ diagram. The crosses mark the position of the main sequence (MS) without extinction at a distance of 1.0 kpc (Tokunaga 2000, Drilling \& Landolt 2000, Martins \& Plez 2006). The reddening curves for an O3 and a F0 star are shown with dashed lines. Sources with high infrared excess have been identified by the corresponding numbers and letters.}}
\end{figure*}

 In order to find primary indicators of stellar formation activity in the region under study, we used the MSX6C Infrared Point Source Catalogue (Egan \etal2003) in Bands  A (\hbox{8.3 $\,\umu$m} ), C (\hbox{12.1 $\,\umu$m}), D (\hbox{14.7$\,\umu$m}), and E (\hbox{21.3$\,\umu$m}); the 2MASS All-Sky Point Source Catalogue (Cutri \etal2003) in bands $J$ (1.25 $\,\umu$m), $H$ (1.65 $\,\umu$m), and $Ks$ (2.17 $\,\umu$m); and the IRAS Point Source Catalogue \footnote{1986 IRAS catalogue of Point Sources, Version 2.0 (II/125)}. In addition, broadband mid- and far-infrared data supplied by the MSX and IRAS satellites were employed to show the large scale distribution of the dust. Star formation activity was investigated within a box centered at \hbox{{\it (l,b)} = (148\degr 45\arcmin, --0\degr 45\arcmin)} of 2\fdg5~in side.

 $^{12}$CO(1---0) data from Dame, Hartmann \& Thaddeus~(2001) were also used to compare the spatial distribution of the tracers of stellar formation activity with that of the molecular gas. These data have an angular resolution of 8.3 arcmin, a velocity resolution of 1.3 km\,s$^{-1}$, and an rms noise of 0.05 K.

The criteria used to identify YSO candidates are described in the following paragraphs.

\subsection{IRAS sources}

A total of 89 IRAS point sources were found projected onto the analyzed region. Junkes, F\"{u}rst \& Reich (1992)'s conditions for young stellar objects are: S$_{100}$ $\ge$ 20 Jy, \hbox{1.2 $\leq$ $\frac{S_{100}}{S_{60}}$ $\leq$ 6.0}, $\frac{S_{100}}{S_{60}}$ $\ge$ 1, and Q$_{60}$+Q$_{100}$ $\ge$ 4, where S$_{\lambda}$ and Q${_\lambda}$ are the flux density and the quality of the IRAS fluxes in each of the observed bands, respectively. Only 7 of the 89 sources can be classified as protostellar candidates following the above mentioned criteria.

\subsection{MSX sources}

The sources were classified based on Lumsden \etal(2002)'s criteria, which allow to select sources taking into account their loci in the (F$_{21}$/F$_{8}$, F$_{14}$/F$_{12}$) diagram. F$_{\lambda}$ denotes the flux in each band. Massive young stellar object (MYSO) candidates have \hbox{F$_{21}$/F$_{8}$ $\ga$ 2} and \hbox{F$_{14}$/$F_{12}$ $\ga$ 1}, while compact \hii regions (CH\,{\sc ii})~present \hbox{F$_{21}$/F$_{8}$ $\ga$ 2} and \hbox{F$_{14}$/$F_{12}$ $<$ 1}. Evolved stars occupy the region \hbox{F$_{21}$/F$_{8}$ $\leq$ 2} and \hbox{F$_{14}$/F$_{12}$ $\leq$ 1}.

 A total of 128 MSX sources are projected onto the whole region. Most of the sources are detected only in the highest sensitivity Band A, while 4 per cent of the sources are detected in Band E. For the case of Bands  C and D, 15 per cent of the sources reach the detection limit of the instrument. Of the detected sources, 20 per cent and 33 per cent have reliable fluxes (corresponding to quality flags 3 or 4) in Bands C and D, and in Band E, respectively. Only the sources detected in Bands A and E are included in the present analysis. Among the sources with reliable fluxes, only one can be catalogued as MYSO candidate. Other two sources, which are not detected in Band C, can be classified as young stellar objects, but their identification as MYSO or CHII remain uncertain.

\subsection{2MASS sources}

 A total of 6548 sources were selected from the 2MASS catalogue. These sources have a photometric quality \hbox{{\it Qflg} = AAA}\footnote{JHK Photometric quality of AAA means [jhk]~snr $\ga$10 and [jhk]~cmsig $\la$ 0.10857 and $Ks$ $<$ 12. The condition imposed on Ks allows to reduce source contamination from field stars with spectral types later than F0. This criterium is also compatible with the purpose of this search, which is to identify YSO candidates with high and intermediate masses.} Mean errors are 0.024, 0.03, and 0.023 mag for J, H, and Ks magnitudes, respectively. The nature of the sources can be inferred from their position in the \hbox{($H-Ks$,$Ks$)} CM and \hbox{($H-Ks$,$J-H$)} CC diagrams. Following Comer\'on \& Pasquali (2005), we define the parameter {\it q} as:

\begin{equation} \label{factorq}
q= (J-H) - 1.83 \times (H-Ks)
\end{equation}

This parameter allows identification of sources in different evolutionary stages. Main sequence stars have q-values in the range --0.15 to 0.10, while sources with infrared excess, like YSOs, have q $\la$ --0.15. For giant stars, q $\ga$ 0.10.\\
\indent The selection criteria described above were applied to the Sh2-205 area and to a control field. The last one is centered at {\it (l,b)} = (146\degr 45\arcmin,--0\degr 45\arcmin) with 2\fdg5 $\times$ 2\fdg5 in size. We believe its stellar population is dominated by field stars. Figure 2 shows the CC (upper left panel) and CM (bottom panel) diagrams for main sequence star candidates and sources with infrared excess found towards Sh2-205. The CC diagram of the control field is presented in the upper right panel of Figure 2. The reddening vectors for early type (O6-8 V) and late-type (M0 III) stars (Koornneef 1983) are represented by two parallel lines in the CC diagrams using extinction values from Rieke \& Lebofsky~(1985). The position of the main sequence at a distance of 1.0 kpc is indicated by the crosses in the ($H-Ks$,$Ks$) diagram.\\

Towards Sh2-205 we found 41 sources with infrared excess (triangles in Fig. 2), 1082 main sequence stars (represented by squares in the CM diagram of Fig. 2), and 5425 giant stars (not included in the plot). In the CC diagram corresponding to Sh2-205, several sources located just below the reddening curve for an O6-8 V star, having q-values close to 0.1 (not shown in the plot), were included as main sequence star candidates. As regards the control field, we found 23 sources with infrared excess, around half the number identified towards Sh2-205. These sources did not show any spatial clustering. On the contrary, some spatial clustering was found toward Sh2-205 (see Section 3). We note that some of the sources with infrared excess which are situated very close to the reddening vector,
especially at low extinctions, might be early-type stars with small photometric errors, moderate
deviations of the actual reddening law from the adopted one or
intrinsic scatter in the colors of early-type stars. If this were the case, the diagram woulb be indicating an excess of early-type stars, probably related to the HII region. The condition for Ks-magnitudes causes a region lacking sources in the CM diagram between Ks = 12 and the reddening curve for a F0 star, thus underestimating the number of Herbig Ae/Be candidates in the analyzed region.

\begin{figure*}
\includegraphics[angle=0,width=0.7\textwidth]{sf-all.eps}
\caption{\small{{\it Left panel}: YSO candidates superimpossed onto the molecular emission averaged within the velocity range [--0.65, --11.1] km\,s$^{-1}$.  Contour levels are 0.5, 1.0, 1.5 K, and  from 3 to 15 K in steps of 2 K. {\it Right panel}: YSO candidates overimpossed onto the emission at 1420 MHz. Contour levels are from 5.3 to 6.1 K in steps of 0.2 K. 2MASS, IRAS, and MSX candidates are indicated by triangles, crosses, and circles, respectively. HD\,2431 and HD\,24094 are identified by nine pointed stars. The box indicates the position of NGC\,1444.}}
\end{figure*}

The CC diagram shows a group of four MS star candidates which has the highest values of visual extinction (A$_{v}$ $\approx$ 15 mag). One of them, named Kiso C5-142 in the Simbad database, with values \hbox{($H-Ks$, $J-H$) = (0.89, 1.71)}, and the source with high infrared-excess named Kiso C5-155, with \hbox{($H-Ks$, $J-H$) = (1.47,1.97)}, are actually carbon stars (Alksnis \etal2001). The nature of the other two MS star candidates will be discussed in the following section.

\section{Distribution of YSOs}

In this section, we will examine the spatial distribution of the detected YSO candidates.

Figure 3 shows an overlay of the $^{12}$CO emission distribution in the velocity range [--0.65, --11] km\,s$^{-1}$~(left panel) and the 1420~MHz image (right panel) and the probable tracers of stellar formation activity. IRAS, MSX, and 2MASS candidates are indicated as crosses, circles, and triangles, respectively. To associate an IR source to a certain \hii region or interstellar bubble within the area under study we considered its proximity to the structure and its correlation with the neutral/ionized associated gas.  We are aware of the fact that no distance information is available in most of the cases. The condition Ks $<$ 12, for the 2MASS sources implies an upper limit to the distance of the sources. The adopted Ks value indicates that we can see an O3 type star with $A_{v} \approx~60~{\rm mag}$ and a B5 type star with $A_{v} \approx~20~{\rm mag}$ at a distance of 1.0 kpc. We discuss our results for the four regions, LBN\,148.11--0.45, \hbox{SH\,148.83--0.67}, \hbox{SH\,149.0--1.30}, and the H\,{\sc i}~shell, separately.

\subsection{Stellar formation in LBN\,148.11--0.45}

\begin{figure*}
\label{fig:sf}
\includegraphics[angle=0,width=0.7\textwidth]{sf-lbn.eps}
\caption{\small {\it Left panel}: Image at \hbox{8.3$\,\umu$m}. YSO candidates from 2MASS, IRAS, and MSX sources are indicated by triangles, crosses, and circles, respectively. HD\,24094 is identified by a nine-points star. MS candidates are indicated by squares.{\it Top right panel}: \hbox{100$\,\umu$m} image ({\it grayscale}) and  $^{12}$CO emission distribution ({\it contours}) within the velocity range [--0.65, --11.1] km\,s$^{-1}$. Contour levels are 1.0, 1.5 K, and from 2.0 to 6.0 K in steps of 1 K.{\it Bottom right panel}: Overlay of the \hbox{100$\,\umu$m} image ({\it grayscale}) and $^{12}$CO emission distribution ({\it contours}) within the velocity range [--31.9, --35.8] km\,s$^{-1}$. Contour levels are from 1.0 to 2.5 K in steps of 0.5 K.}
\end{figure*}

The distribution of gas and dust in the environs of \hbox{LBN\,148.11--0.45} is shown in Fig. 4. The left panel shows the YSO candidates in the environs of \hbox{LBN\,148.11--0.45} superimpossed onto the emission at 8.3$\,\umu$m. Numerous infrared objects are seen projected onto this region. 2MASS, IRAS, and MSX candidates are indicated by triangles, crosses, and circles, respectively.

The top right panel displays an overlay of the $^{12}$CO(1--0) emission distribution ({\it contours}) in the range \hbox{[--0.65, --11.1]} km\,s$^{-1}$~and the infrared emission at \hbox{100$\,\umu$m} ({\it grayscale}), while the bottom right panel depicts an overlay of the $^{12}$CO(1--0) emission distribution ({\it contours}) in the range [--31.9, --35.8] km\,s$^{-1}$~and the \hbox{100$\,\umu$m} image.

Properties of IRAS, MSX, and 2MASS sources are listed in the Table 1. The designation of the IRAS sources, {\it (l,b)} positions, fluxes at 12$\,\umu$m, 25$\,\umu$m, 60$\,\umu$m, and 100$\,\umu$m, luminosities derived following Yamaguchi \etal (1999), and association with other sources, along with a reference number, are indicated in the table. For the MSX sources we included the candidate designation, the {\it (l,b)} position, the fluxes at 8.3$\,\umu$m, 12.1$\,\umu$m, 14.7$\,\umu$m, and 21.3$\,\umu$m, and the association with other sources. The quality flag of the sources in each band, Q$_{\rm flag}$,  appears indicated in Col. 8 with numbers from 0 to 4. While "0" means that the source has not been detected, "1" to "4" indicate a better detection of the source as the number increases. Identification as MYSO or CHII is included. As regards 2MASS candidates, names, {\it (l,b)} positions, fluxes in the 2MASS IR wavelengths, colours $(J-H)$ and $(H-Ks)$, and association with other sources, are listed.

This region can be divided in two areas based on the distribution of the YSO candidates: one close to {\it (l,b)} = (148\degr, +0\degr 15\arcmin) and the other near \hbox{LBN\,148.11--0.45} itself (see Fig. 4).

Twelve candidates are projected near {\it (l,b)} = (148\degr, +0\degr15\arcmin). An inspection of the image at 100$\,\umu$m, shows that the candidates coincide with filamentary emission. This extended feature is not detected at 8.3$\,\umu$m. At this wavelength, only knots of bright emission coincident with the sources are identified.

The YSO candidates are found projected onto the molecular cloud detected in the velocity range \hbox{[--31.9,--35.8] km\,s$^{-1}$}~(see Fig 3, bottom right panel). The source IRAS\,03523+5343 (IRAS $\#$2) was associated with molecular gas detected in $^{12}$CO at \hbox{v = --34.6 km\,s$^{-1}$} by Wouterloot \& Brand (1989), who derived a kinematical distance d$_{k}$ $\approx$ 4.2 kpc. Adopting this distance, the infrared luminosity of the source is 6500  L$_{\sun}$ (Yamaguchi \etal 1999). One can wonder whether this star forming region might be an outflow of the \hii\ region LBN\,14811--0.45, and consequently be placed at the same distance. The presence of molecular emission with velocities in the range [--0.65,--11.1] km\,s$^{-1}$~bordering the ionized region at b --0\degr 10\arcmin\ casts doubts on this interpretation. On the other hand, if the molecular cloud at --34 km\,s$^{-1}$~were located at the distance of the
\hii\ region, this cloud would have an approaching velocity of at least 25 km\,s$^{-1}$,
while we would expect a radial velocity closer than the systemic velocity of the
\hii\ region for a champagen flow. Moreover, radio emission from
the ionized gas
in the region between LBN\,14811--0.45 and the star forming area, which
should be present in a champagne flow, is absent.

IRAS\,03529+5345 (IRAS $\#$1) is almost coincident in position with a nebular object present in the NGS-PO Sky Survey and called RNO22 by Cohen (1980), who established from an optical spectrum that it was a F5 star, with relatively high reddening. Based on this
classification and in the apparent magnitude \hbox{m$_{v}$ = 15.3 mag} and visual extinction given by the author, and taking into account \hbox{M$_{v}$ = 3.5 mag} (Drilling \& Landolt 2000), we estimated a distance of \hbox{$\approx$ 500 pc} for the F5 star.
On the other hand, a chance superposition can not be ruled out. Moreover, the presence of other evidences of active stellar fomation 4\arcmin\ far from IRAS $\#$1 located at larger distances casts doubts on the association of the IRAS source and the F5 star.

As regards IRAS\,03517+5340 (IRAS $\#$3), no additional information is found in the literature. It is also probably related to molecular gas at --33 km\,s$^{-1}$. If located at 4.2 kpc, its infrared luminosity also suggests a massive object.

MSX sources $\#$4 and $\#$5 and 2MASS sources $\#$7 and $\#$8 are almost coincident with IRAS
$\#$2, while 2MASS sources $\#$9 and $\#$11 are projected onto the position of IRAS $\#$3. MSX source $\#$6 and 2MASS source $\#$12 are close to the last group. Note that $\#$8, $\#$9, and $\#$12 are among the sources with the highest infrared excess (see Fig. 2). Source $\#$10 is also probably connected to the star forming region at d $\approx$ 4.2 kpc.

As regards, LBN\,148.11--0.45, the 2MASS sources $\#$13 to $\#$18 are placed close to the ionized border. They are projected onto the molecular structure detected within the range \hbox{[--0.65,--11.1]} km\,s$^{-1}$. Sources $\#$13, $\#$14, $\#$16, and $\#$18 appear projected onto the outer border of the PDR, marked by the emission at 8.3$\,\umu$m (see Fig. 4, left and top right panels).

The 2MASS source $\#$16 has the highest infrared excess in the region [($H-Ks$, $J-H$) = (1.78,2.55)]. It is projected onto the PDR, close to the brightest CO emission region. No additional information on the 2MASS YSO candidates is found in the literature.

 The MSX knot at {\it (l,b)} = (148\degr 0\arcmin,--0\degr 10\arcmin) is an interesting object. As found in Paper I, it is 1.5 arcmin far from the radio continuum point source \hbox{NVSS\, J035327+533601}, which is a non-thermal, probably extragalactic source. Flux densities for this source are 45$\pm$27 mJy and 13$\pm$0.9 mJy at 408 MHz and 1420 MHz, respectively, and  the spectral index is --1.00$\pm$0.2 (Paper I).
 A total of 5 main sequence candidates are projected onto this knot of emission. They are listed in the bottom part of Table 1. Sources $\#$a and $\#$b have the highest visual extinction among the complete set of main sequence stars. It would be interesting to investigate the true nature of this object.

The difference in distance between the \hii region LBN\,148.11--0.45 and IRAS $\#$2 and $\#$3 suggests that we have identified two independent star forming regions, without apparent physical relation. IRAS $\#$1 is a late type star seen projected onto the environs of \hbox{LBN\,148.11--0.45}, without physical association either with the \hii region or the star forming area at 4.2 kpc.

To sum up, we have identified two star forming regions: one near (l,b) = (148\degr 0\arcmin, +0\degr 15\arcmin) and the other connected to \hbox{LBN\,148.11--0.45}.

As regards the first area, placed at d $\approx$ 4.2 kpc, eleven primary tracers were identified. Six YSO candidates were found in the environs of \hbox{LBN\,148.11--0.45}. Most of them located in the PDR.

\begin{table*}
\label{table:r1}
\begin{center}
\small
\vspace{3mm}
\caption{\small{YSO candidates from the IRAS, MSX, and 2MASS catalogues towards LBN\,148.11--0.45}}
\begin{tabular}{@{}clllrrrrcc}
\hline\hline
\multicolumn{9}{c}{{\bf IRAS sources}} \\
 $\#$ &  Designation &  {\it (l,b)}&     \multicolumn{4}{c}{Fluxes [Jy]}  & $L_{IRAS}$ &Comments\\
             &                         &[$\circ\ \arcmin$,$\circ\ \arcmin$]     &  12$\mu$m  &    25$\mu$m &   60$\mu$m &  100$\mu$m &$[L_{\sun}]$  &\\
\hline
1 & 03529+5345 & 148\degr   9\farcm3 +0\degr  22\farcm32 & 1.4 &1.2     & 13.4 & 40 &18 $\dag$&RNO 22\\
2 & 03523+5343 & 148\degr   7\farcm2  +0\degr  17\farcm52 & 6.1 &30.8 & 87.2 &151 &6500$\dag$ $\dag$ &$\#$4, $\#$5, $\#$7, $\#$8 \\
3 & 03517+5340 & 148\degr  5\farcm04  +0\degr  11\farcm28 & 0.5 &0.5 & 5.7& 31.9 &800$\dag$ $\dag$ &$\#$9, $\#$11\\
\hline
\hline
\multicolumn{9}{c}{{\bf MSX sources}} \\
 \hline
  $\#$ &  Designation  &    {\it (l,b)}&     \multicolumn{4}{c}{Fluxes [Jy]}  & Q$_{\rm flag}$ &Comments\\
        &                           &[$\circ\ \arcmin$,$\circ\ \arcmin$]    &  \hbox{8.3$\,\umu$m}  &  \hbox{12.1 $\,\umu$m} & \hbox{14.7$\,\umu$m} & \hbox{21.3$\,\umu$m} &ACDE  &\\
\hline
\multicolumn{9}{c}{{\bf MYSO candidate}}\\
4 &G148.1201+00.2928 & 148\degr  7\farcm2  +0\degr  17\farcm58 & 3.01 & 6.21 & 8.96 & 21.47 &  4444&$\#$2, $\#$5, $\#$7, $\#$8 \\
 \multicolumn{9}{c}{{\bf Compact \hii region/MYSO candidates}}\\
5 &G148.0930+00.2783 & 148\degr  5\farcm58  +0\degr  16\farcm68 & 0.48 & ... & 0.67 & 2.65 &4013& $\#$2, $\#$4, $\#$7, $\#$8  \\
6&G148.1042+00.1383 & 148\degr  6\farcm4  +0\degr 8\farcm28 & 0.44 & ... & 1.09 & 2.64 & 4011& $\#$12\\
  \hline
\hline
\multicolumn{9}{c}{{\bf 2MASS sources}} \\
\hline
$\#$ & Designation  & {\it (l,b)} [$\circ\ \arcmin$,$\circ\ \arcmin$]&     $J$& $H$ & $Ks$ & $(J-H)$& $(H-Ks)$ &Comments\\
 \hline
 7&03561628+5353025 & 148\degr  6\farcm78  +0\degr  18\farcm3 & 13.62 & 12.43 & 11.67 & 1.19 &0.76 & $\#$2, $\#$4, $\#$5, $\#$8 \\
 8&03560333+5352352 & 148\degr  5\farcm63  +0\degr  16\farcm74 & 13.30 & 11.01 & 9.31 & 2.29& 1.70 & $\#$2, $\#$4, $\#$5, $\#$7\\
 9&03554277+5350074 & 148\degr  4\farcm86  +0\degr   12\farcm54 & 13.92 &  12.48  & 10.82& 1.44&  1.658 &   $\#$3, $\#$11\\
10&03551336+5352390 & 147\degr  59\farcm93  +0\degr  12\farcm06 & 11.63 & 10.97 & 10.49 & 0.65 & 0.48 & \\
11&03554527+5348408 & 148\degr  6\farcm12  +0\degr  12\farcm06 & 13.73 & 12.44 & 11.56 &  1.28 & 0.88 &$\#$3, $\#$9\\
 12&3553004+5345419 & 148\degr  6\farcm30  +0\degr  8\farcm34 & 12.55 & 10.92 & 9.65 & 1.63 &1.27 &$\#$6 \\
13&03540902+5346002 & 147\degr  56\farcm88  +0\degr  0\farcm9 & 10.24 & 9.59 & 9.107 & 0.64&0.49 & \\
 14& 03553869+5315396 &     148\degr  26\farcm52 --0\degr 13\farcm92 & 11.19&  10.83&  10.46&0.37&0.36\\
15&03534163+5308487 & 148\degr  17\farcm39  --0\degr  30\farcm36 & 12.71 & 11.60 & 10.83 & 1.11&0.77 & \\
16&03532733+5308127 & 148\degr  16\farcm07  --0\degr  32\farcm22 & 10.85 & 8.30 & 6.53 & 2.55&1.78 & \\
17&03512640+5322413 & 147\degr  52\farcm92  --0\degr  32\farcm46 & 13.96 & 12.94& 11.91 & 1.02&1.03 & \footnotesize{NVSS\, J035327+533601} \\
 18&03505606+5311217 & 147\degr  56\farcm52  --0\degr  44\farcm1 & 12.67 & 12.03 & 11.59 & 0.64&0.44 & \\
\hline
\multicolumn{9}{c}{{\bf MS candidates towards {\it (l,b)} $\approx$ (148\degr ,--0\degr 10\arcmin)}} \\
a&03533411+5336223&147\degr 58\farcm98 --0\degr 9\farcm84 & 12.56 & 10.83 & 9.83 & 1.73 & 0.99 &\\
b&03534258+5335290&148\degr 0\farcm54 --0\degr 9\farcm72 & 12.72 & 11.43 & 10.74 & 1.29 & 0.69 &\\
c&03533521+5336575&147\degr 58\farcm74 --0\degr 9\farcm24 & 12.25 & 10.69 & 9.79 & 1.56 & 0.89 &\\
d&03534224+5334591&148\degr 0\farcm84 --0\degr 10\farcm14 & 11.57 & 10.78 & 10.35 & 0.79 & 0.43 &\\
e&03533002+5334396 &147\degr 59\farcm64 --0\degr 11\farcm52& 12.71 &12.02& 11.66 &0.69&0.37 &\\
\hline
\hline
\end{tabular}
\end{center}
$\dag$: Calculated adopting a distance of 500 pc\\
$\dag$ $\dag$: Calculated adopting a distance of 4200 pc\\
\end{table*}

\subsection{Stellar formation in SH\,148.83--0.67 and in SH\,149.25--0.00}

Protostellar objects associated with this region are listed in Table 2, which is organized in the same way as Table 1. Figure 3 shows several 2MASS candidates projected onto the radio continuum emission at 1420 MHz. No IRAS and MSX candidates are found in this region.

Eight YSO candidates were found in this region. Fig. 3 shows the spatial distribution of the candidates onto the atomic neutral gas structure associated with SH\,148.83--0.67 (Paper I). This figure shows the 21--cm HI line emission within the velocity range \hbox {[--25.0,--28.0]} km\,s$^{-1}$~(Paper I).  Source $\#$26 coincides with the radio continuum point source NVSS~J035347+523208, which  is  probably a pulsar. Flux densities for this source are 33$\pm$16 mJy and 1.94$\pm$0.25 mJy at 408 and 1420 MHz, respectively. The spectral index is --2.27$\pm$0.68 (Paper I).

To summarize, the 2MASS sources are projected onto the HI low emision region and are characterized by low infrared excess compatible with the lack of related molecular and dust emission. This fact casts doubts on the nature of the sources. 2MASS sources $\#$20 and $\#$23 (see Table 2) coincide with HBHA\,5215-03 and HBHA\,5215-01, two emission-line stars (Kohoutek \& Wehmeyer~1999). No additional data about these sources are found in the literature.

\begin{figure}
\includegraphics[angle=0,width=0.50\textwidth]{SH148-HI-YSOS.EPS}
\caption{\small{YSO candidates overimpossed onto the atomic neutral gas emission distribution associated with SH\,148.83--0.67. The map shows the HI emission distribution in the velocity range from --25.0 to --28.0 km\,s$^{-1}$. Contour levels are from 60 to 100 K in steps of 10 K. 2MASS candidates are indicated by triangles. HD\,24431 is identified by a nine pointed star.}}
\end{figure}

As regards SH\,149.25--0.00, five 2MASS and one IRAS candidates were found in this region (Table 3). IRAS source \#27 is associated with DSH\,J0402.3+5226. This source was identified as an infrared cluster by Kronberger \etal(2006), reinforcing its identification as a stellar formation tracer. YSO candidates associated with this nebula are listed in Table 3, where the information is organized as in Table 1.
Additional data  for these sources were not found in the liturature.

In summary, eight candidates were found towards SH\,148.83--0.67, and six ones were identified towards SH\,149.25-0.00.
The lack of molecular gas linked to these sources strengthens the uncertainty in their true nature.

\begin{table*}
\centering
\small
\vspace{3mm}
\caption{\small{YSO candidates from 2MASS catalog towards SH\,148.83--0.67.}}
\begin{tabular}{@{}rllcrrrrcc}
\hline
\hline
\multicolumn{9}{c}{{\bf 2MASS sources}} \\
\hline
$\#$ & Designation  &{\it (l,b)} [$\circ\ \arcmin$,$\circ\ \arcmin$]&     $J$& $H$ & $Ks$ & $(J-H)$& $(H-Ks)$ &Comments\\
 \hline
19&03581253+5254467 & 148\degr  57\farcm6 --0\degr  15\farcm0 & 11.51 & 11.41 & 11.22 & 0.09 &0.19 &  \\
20 &03581379+5243109 & 149\degr  5\farcm27  --0\degr  23\farcm76 & 11.64 & 11.17 & 10.76 & 0.47 &0.41 &  HBHA 5215-03\\
21&03565522+5251200 &148\degr 50\farcm94 --0\degr 25\farcm2&  12.03 & 11.43  &10.89&0.59&0.54&\\
22&03564905+5247384&148\degr 52\farcm62 --0\degr 28\farcm62&  12.47&  11.94&  11.50&0.53&0.44&\\
23&03552988+5247463 &148\degr 43\farcm38 --0\degr 36\farcm18&  11.57&  10.82&  10.26&0.75&0.55&HBHA 5215-01\\
24&03573712+5230068 & 149\degr  9\farcm48  --0\degr  37\farcm32 & 11.37 & 10.61 & 9.75 & 0.76 &0.86 & \\
25&03561414+5226030 & 149\degr  2\farcm46 --0\degr 48\farcm54 & 10.89 & 10.58 & 10.26 & 0.32 & 0.32 & \\
26&03535289+5231356 & 148\degr  42\farcm35  --0\degr  58\farcm02 & 12.66 & 11.76 & 11.17 & 0.90 &0.59 & \footnotesize{NVSS~J035347+523208} \\
\hline
\hline
\end{tabular}
\end{table*}

\begin{table*}
\centering
\small
\vspace{3mm}
\caption{\small{YSO candidates from the IRAS and 2MASS
catalogues towards SH\,149.25--0.00.}}
\begin{tabular}{@{}rllrrrrcc}
\hline\hline
\multicolumn{9}{c}{{\bf IRAS sources}} \\
 $\#$ &  Designation & {\it (l,b)}&     \multicolumn{4}{c}{Fluxes [Jy]}  & $L_{IRAS}$ &Comments\\
             &                         &[$\circ\ \arcmin$,$\circ\ \arcmin$]     &  12$\mu$m  &    25$\mu$m &   60$\mu$m &  100$\mu$m &$[L_{\sun}]$  &\\
\hline
27 & 03584+5217 & 149\degr   44.22  --0\degr  12.72 & 1.4& 3.6 & 41.5& 91.1 & 168&DSH\,J0402.3+5226\\
 \hline
\hline
\multicolumn{9}{c}{{\bf 2MASS sources}} \\
\hline
$\#$ & Designation  & {\it (l,b)} [$\circ\ \arcmin$,$\circ\ \arcmin$]&     $J$& $H$ & $Ks$ & $(J-H)$& $(H-Ks)$ &\\
 \hline
28 &04011799+5331341&148\degr 54\farcm72  +0\degr 30\farcm96  &10.06 & 9.88 & 9.7&0.18&0.18&\\
29&04012921+5321001 & 149\degr  2\farcm88  +0\degr  24\farcm12 & 11.94 & 11.54 & 11.24 & 0.40 &0.30 & \\
30&04011993+5311221 & 149\degr  8\farcm16  +0\degr  15\farcm9 & 11.14 & 10.51 & 10.02 & 0.63 & 0.49 & \\
31&03595517+5228084&149\degr 26\farcm78 --0\degr 25\farcm14&  12.31 & 12.12&  11.93&0.19&0.19&\\
32&04014039+5236281 & 149\degr  33\farcm42 --0\degr  8\farcm4 & 12.15 & 11.72 & 11.39 & 0.42 &0.34 & \\
\hline
\hline
\end{tabular}
\end{table*}

\subsection{Stellar formation in the H\,{\sc i}~shell centered at \hbox{{\it (l,b)} = (149\degr 0\arcmin, --1\degr 30\arcmin)}}

\begin{table*}
\centering
\small
\vspace{3mm}
\caption{\small{YSO candidates from 2MASS catalog towards the H\,{\sc i}~shell centered at \hbox{{\it (l,b)} = (149\degr 0\arcmin, --1\degr 30\arcmin)}}}
\begin{tabular}{@{}rllcrrrrcc}
\hline\hline
\multicolumn{9}{c}{{\bf IRAS sources}} \\
 $\#$ &  Designation &  {\it (l,b)}&     \multicolumn{4}{c}{Fluxes [Jy]}  & $L_{IRAS}$ &Comments\\
             &                         &[$\circ\ \arcmin$,$\circ\ \arcmin$]     &  12$\mu$m  &    25$\mu$m &   60$\mu$m &  100$\mu$m &$[L_{\sun}]$  &\\
\hline
33&03494+5204& 148\degr 49\farcm80 --01\degr 15\farcm90&1.1&1.2 &3.9& 20.2&---&CPM\,10, $\#$37\\
34&03530+5117& 149\degr 47\farcm12 --01\degr 31\farcm26&0.8&0.9&10.5&32.5&55&GN\,03.53.0\\
\hline
\hline
\multicolumn{9}{c}{{\bf 2MASS sources}} \\
\hline
$\#$ & Designation  &{\it (l,b)} [$\circ\ \arcmin$,$\circ\ \arcmin$]&     $J$& $H$ & $Ks$ & $(J-H)$& $(H-Ks)$ &Comments\\
 \hline
35&03511239+5256253& 148\degr 07\farcm86  --00\degr 54\farcm18& 11.94 & 11.80  &11.63&0.14&0.17&\\
36&03503912+5239564&148\degr 14\farcm28 --01\degr 10\farcm14&11.16 & 11.11&  10.96&0.05&0.15&\\
37&03531598+5213009 & 148\degr 49\farcm80 --01\degr 15\farcm90 & 12.35&  11.38&  10.43&0.98&0.94&CPM 10, $\#$33\\
38 &03502506+5228548& 148\degr 19\farcm50 --01\degr 19\farcm80&   6.17 & 6.12&  5.99&0.05&0.12&HD\,23800 \\
39 &03502972+5223315&  148\degr 23\farcm46 --01\degr 23\farcm46 & 13.35 & 12.42&  11.83&0.92&0.59&\\
40 &03473627+5237006&  147\degr  54\farcm42 --01\degr 29\farcm76 &12.43  &12.20 & 11.99&0.23&0.22&\\
41&03541653+5132575&   149\degr 22\farcm50 --01\degr 40\farcm92&7.92&  7.91&  7.82&0.001&0.09&HD\,24275\\
42&03585445+5209145 & 149\degr 32\farcm04  --00\degr 45\farcm54 & 11.83&  11.77&  11.59&0.059&0.17&\\
 \hline
\hline
\end{tabular}
\end{table*}

Based on the criteria mentioned in Sect.3, two IRAS and eight 2MASS candidates are projected in the environs of the H\,{\sc i}~and CO shells. They are listed in Table 4.

Source $\#$34 was associated with the reflection nebula GN\,03.53.0 by Magakian~(2003).

IRAS source $\#$33 was identified by Campbell, Persson \& Matthews (1989) as an YSO candidate based
in its colours ($H-Ks$,$J-H$). Its near-infrared counterpart is 2MASS $\#$37. Its distance is unknown. This source is projected onto the void of molecular emission, suggesting that this object is unconnected to the H\,{\sc i}~shell.

 2MASS sources $\#$38 and $\#$41, which are projected close to the inner border of the molecular ring, were identified as the  near-infrared counterpart of HD\,23800 (B1.5 IVe, Hiltner 1956) and HD\,24275 (A3 V, Rydstrom~1978), respectively. These sources have low infrared excess and lie in the bottom left section of the ($H-Ks$,$J-H$) diagram (Fig. 2), where objects in different evolutionary stages are found (Lada \& Adams 1992).

There is a group of six 2MASS sources with \hbox{{\it l} $\le$ 149\degr 30\arcmin}~(see Fig. 3) which are projected onto the outer border of the molecular ring. These sources may be a connected to Sh2-206, located at \hbox{{\it (l,b)}  = (150\degr 36\farcm18, --00\degr 56\farcm52)}, of 50 arcmin in diameter. Sh2-206 is a blister \hii region catalogued as a star-forming region (Mookerjea \etal 1999). Up to present, neither near nor mid-infrared systematic study was performed to search for  stellar formation tracers in this region. However, the positions of these 2MASS sources suggest that they may be associated with Sh2-206.

To sum up, five YSO candidates probably related to the H\,{\sc i}~and CO shell were identified.

\section{Discussion}

MSX emission at \hbox{21.3$\,\umu$m} is essential to detect embedded sources
in molecular clouds (e.g Rathborne et al. 2004). However, the least
sensitivity in  Band E makes it difficult to detect sources at
\hbox{21.3$\,\umu$m}. This fact leads us to underestimate the number of MSX
point sources since only sources detected in both Bands A and E have been
taken into account. Additionaly, only 20-30 per cent of the YSOs can be identified by using 2MASS CC and CM diagrams, as Nielbock, Chini \& M\"uller~(2003) found in the star forming regions OMC 2 and 3. As a consequence, the number of candidates in our analyzed regions is understimated.

Taking into account these constraints, \hbox{LBN\,148.11--0.45} shows a noticeable interesting scenario. The YSO candidates are found in the periphery of the optical nebula, onto or close to the PDR and embedded in the molecular gas. Besides, the age the \hii region (\hbox{4 $\times$ 10$^{6}$ yr}, Paper I) is compatible with the existence of Class I sources (Andr\'e \etal 2000).

This \hii region is evolving in an interstellar medium with an original ambient density of $\approx$ $800~cm^{3}$ (Paper I). These results open the question whether this region is another example of triggered star formation in our Galaxy. The "collect and collapse" model indicates that the expansion of \hii regions on their surroundings creates compressed layers where gas and dust are piled-up between the ionization and the shock fronts. The latter fragmentation of the collected layer ends forming molecular cores where new stars born. The analytical model developed by Whitworth \etal(1994) analyzed the consequences of the dynamical instabilities occurred in the collected layer. They considered three different scenarios where the fragmentation can occur: expanding \hii regions, stellar wind bubbles, and supernova remmants. In all cases, they found that the resulting fragmentation in the shocked layers generates high mass clumps (i.e. $\ge~7~{\rm M}_{\odot}$) which are initially well separated.

For the case of \hii regions, the theory predicts the time at which the fragmentation occurs, $t_{frag}$, the size of the \hii region at that moment, $R_{frag}$, the column density of the shell when the process begins, $N_{frag}$, the mass of the fragments, $M_{frag}$, and their separation along the layers, $r_{frag}$. The parameters required to derive these quantities are the number of Lyman continumm photons emitted per second by the exciting sources, ${\it N}_{Ly}$, the ambient density of the surrounding medium into which the \hii region expands, n$_{0}$, and the isothermal sound speed in the shocked gas, $a_{s}$, which is supposed to be constant.

The analytical expressions are:
\begin{equation}
{\it t}_{frag}~[10^{6}~{\rm yr}]~=~1.56~~a_{.2}^{4/11}~~n_{3}^{-6/11}~~N_{Ly}^{-1/11}
\end{equation}

\begin{equation}
{\it R}_{frag}~[{\rm pc}]~=~5.8~~a_{.2}^{4/11}~~n_{3}^{-6/11}~~N_{Ly}^{1/11}
\end{equation}

\begin{equation}
{\it N}_{frag}~[10^{21}~{\rm cm}^{-2}]~=~6.0~~a_{.2}^{4/11}~~n_{3}^{-6/11}~~N_{Ly}^{1/11}
\end{equation}

\begin{equation}
{\it M}_{frag}~[{\rm M_{\odot}}]~=~23~~a_{.2}^{40/11}~~n_{3}^{-5/11}~~N_{Ly}^{-1/11}
\end{equation}

\begin{equation}
2 {\it r}_{frag}~[{\rm pc}]~=~0.83~~a_{.2}^{18/11}~~n_{3}^{-5/11}~~{\rm N}_{Ly}^{-1/11}
\end{equation}

\noindent where $a_{.2}$ $\equiv$ $\frac{{\it a}_{s}}{0.2~km~s^{-1}}$, $n_{3}$ $\equiv$ $\frac{{\it n}_{0}}{1000~cm^{3}}$

These equations show that $a_{s}$ is an important factor to derive the parameters, while  $n_{0}$ has a lower contribution, and the dependence with $N_{Ly}$ is notoriously weak. A remarkable result from eq. 5 is that the mean mass of the fragments increases as the sound speed grows.

For the case of \hbox{LBN\,148.11--0.45}, the parameters $N_{Ly}$ and $n_{0}$ were derived from the free-free radio continuum emission (Paper I). The rate of Lyman continuum photon emission is at least, \hbox{4~$\times~10^{47}~{\rm s}^{-1}$}, and the ambient density, $800~{\rm cm}^{3}$. Whitworth \etal(1994) pointed out that $a_{s}$ is in the range from 0.2 to 0.6 km\,s$^{-1}$. For this \hii\ region, the larger $a_{s}$ values lead to unrealistic parameters. For example, for $a_{s}$  = 0.35 km\,s$^{-1}$, the mass of the fragments increases dramatically ($\approx$ 300 $\rm M_{\odot}$) and their radii reach values larger than the size of the HII region. Acceptable parameters are obtained for the present case by taking into account $a_{s}$ in the range 0.2 to 0.3km\,s$^{-1}$. In the following, we will adopt 0.2 km\,s$^{-1}$, which corresponds to typical temperatures of 10 K for the molecular clouds.

Considering that the radius of the \hii region is $R_{H II}$ = 7.2 pc, and the dynamical age $t_{dyn}$ \hbox{$=$ $4 \times 10 ^{6}$ yrs}, we compare them with the derived parameters (Table 5). According to the table, $R_{frag}$ $<$ $R_{H II}$ and t$_{dyn}$ $>$ $t_{frag}$, indicating that massive molecular fragments were able to form in the environs of LBN\,148.11--0.45. The distance between fragments is lower than the minimum linear size that the angular resolution of CO data allows to separate (i.e. {\it r} = 2.4 pc at a distance of 1.0 kpc). Better angular resolution data and different line transitions are needed to observe the molecular fragments. Other phenomenon of fragmentation can act simultaneously in this zone. Molecular cores can be formed by radiative-driven collapse, namely the called "Radiation-Driven Implosion" (RDI) theorically developed by Lefloch \& Lazareff (1994). Structures such as cometary globules and elephant trumps can be observational examples of this process
(e.g. Lefloch, Lazareff \& Castets 1997). However, the angular resolutions of optical and infrared observations do not allow to identify the presence of these objects. As a consequence, there is neither evidence nor necessary data to apply the RDI model in this region. Thus, none of the two models can be discarded to explain the stellar formation process in the environs of \hbox{LBN\,148.11--0.45}.

\begin{center}
\begin{table}
\caption{Parameters for the the shocked layers in the environs of LBN\,148.11--0.45.}
\vspace{1.5mm}
\begin{tabular}[h!]{lc}
\hline\hline
Parameter&Value\\
\hline\hline
$M_{frag}$~$[M_{\odot}]$ &33\\
$t_{frag}$~$[10^{6}~yr]$& 2.3 \\
$R_{frag}$~[pc]&5\\
$r_{frag}$~[pc]& 0.6\\
$N_{frag}$~[$10^{21}~cm^{-2}$]&4\\
\hline\hline
\end{tabular}
\end{table}
\end{center}

\section{Summary}

We have analyzed the stellar formation activity in four different regions of Sh2-205.

Based on MSX, 2MASS, and IRAS point source catalogues, we have identified YSO candidates in the region by applying criteria by Junkes, F\"{u}rst \& Reich (1992), Lumsden \etal(2002), and using CM and CC diagrams. Additional information was obtained from Simbad database and broadband mid- and far-infrared images supplied by the MSX and IRAS satellites, and $^{12}$CO(1---0) data.

Our main results can be summarized as follows:

\indent 1.~Six of the seven IRAS, thirty of the fourty-one 2MASS, and the three MSX sources identified as YSO candidates were found projected onto the four structures.

\indent 2.~Of these, eight candidates were found towards  \hbox{SH\,148.83--0.67}, and six candidates were identified towards  \hbox{SH\,149.25-0.00}. However, the lack of molecular gas linked to these sources casts doubts on their nature and their physical association to the structures.

\indent 3.~Five YSO candidates probably related to the H\,{\sc i}~and CO shell centered at \hbox{{\it (l,b)} = (149\degr 0\arcmin, --1\degr 30\arcmin)} were identified. The agent responsible of this structure remains unknown.

\indent 4.~In the environs of \hbox{LBN\,148.11--0.45} we have identified two star forming regions: one near (l,b) = (148\degr 0\arcmin, +0\degr 15\arcmin) and the other connected to \hbox{LBN\,148.11--0.45} itself.

As regards the first area, placed at d $\approx$ 4.2 kpc, eleven primary tracers were identified.

Six YSO candidates were found in the environs of \hbox{LBN\,148.11--0.45}. Most of them are situated close to the PDR, projected onto molecular material. By applying Whitworth \etal(1994)'s theorical model to this region we find that the formation of massive fragments would be taking place in this region. Higher angular resolution data are necessary to detect the molecular fragments.

5. Finally, two findings can be highlighted: the presence of tracers of star formation activity found in \hbox{LBN\,148.11--0.45} and the requirement of high UV photon flux necessary to keep this \hii region ionized. The combination of these two facts reinforces the argument that HD\,24094 was miss-classified as a B8-type star (Paper I) and the existence of hidden exciting sources responsible for this stellar formation process.

\section{Future work}

Millimetre observations are needed to confirm whether the fragmentation is ocurring in the environs of \hbox{LBN\,148.11--0.45}. Near- and mid-infrared data are important to detect the embedded sources. Spitzer satellite is much more sensitive and has higher spatial resolution than the infrared surveys used in this work (Werner \etal2004). Particularly, IRAC and MIPS 24 $\mu$m colour-colour diagram ([3.6]-[5.8],[8.0]-[24.0]) provides a good observational tool for determing the evolutionary stage of YSOs (Robitaille \etal2006). Unfortunately, no Spitzer data are available for this region. High-quality Spitzer data would allow a more accurate and comprehensive analysis of star formation activity in the environs of LBN\,148.11--0.45.

\section*{Acknowledgments}

We thank the anonymous referee for suggestions that resulted in substantial improvements to the paper. This paper was partially financed by the
Consejo Nacional de Investigaciones Cient\'{\i}ficas y T\'ecnicas
(CONICET)
of Argentina under project PIP 5886/05, Agencia PICT
14018, and UNLP 11/G093. \\
This research has made use of the NASA/ IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. The MSX mission is sponsored by the Ballistic Missile Defense Organization (BMDO). This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France.

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Suniaire de Pallars (mort en 1011) est comte de Pallars de 948 à sa mort et comte consort de Ribagorce de 1006/1007 à sa mort. Il succède à son père Loup, comte de Pallars.

Biographie

Les origines de Suniaire sont obscures : ni sa date, ni son lieu de naissance ne sont connus. Il est le fils du comte de Pallars Loup et de son épouse Gotrude de Cerdagne. Celle-ci était, par sa mère, la petite-fille des comtes Miron II, comte de Cerdagne et de Besalu, et de Dela, comte d'Ampurias.

À la mort de son père en 948, et à la suite du renoncement de son oncle Isarn de Pallars, le gouvernement du comté passe entre les mains de sa mère, qui exerce le pouvoir pour ses fils. En 963, ses deux frères Raymond II et Borell exercent le pouvoir conjointement, et en 966 Suniaire accède lui aussi à la dignité comtale, conjointement avec eux.

Après la mort en 995 de ses deux frères ainés, le neveu de Suniaire, Armengol, héritier de son frère Borell gouverne alors le Pallars conjointement avec lui. Il épouse, certainement peu après, la veuve de son frère Borell, Ermengarde de Rouergue, dont il a deux fils, Raymond et Guillaume, et une fille, Ermengarde.

Suniaire poursuit la politique de ses frères et soutient les ordres religieux dans son comté. Il confirme la donation du  à l'abbaye de La Grasse en 1006, confirme ses donations au chapitre cathédral d'Urgell en 1010 et reconnait les droits du  sur la villa de Somponiu la même année.

En 1006 ou 1007, il épouse la comtesse de Ribagorce, Toda. Il est avéré qu'il l'accompagne dans l'exercice du pouvoir en Ribagorce. Il fait avec elle des donations au  en 1008. D'après la Chronique II d'Alaó, Suniaire oblige également l'évêque de Ribagorce Aymeric II à reconnaître la supériorité de l'évêque d'Urgell.

En 1011, à la mort de Suniaire, son épouse Toda retourne sur ses terres et cède le pouvoir à son neveu, Guillaume de Ribagorce. Au Pallars, ses deux fils (leur cousin Armengol étant décédé en 1010) se partagent le comté de Pallars selon le vœu de leur père : Raimond obtient le comté de Pallars Jussà et Guillaume le comté de Pallars Sobirà.

Mariages et descendance

Suniaire épouse en premières noces, entre 995 et 1000, Ermengarde de Rouergue, fille du comte de Rouergue Raimond II. Elle était la veuve du frère de Suniaire, Borell. De cette union sont issus :

 Raymond III (?-1047), comte de Pallars Jussà ;
 Guillaume II (?-1035), comte de Pallars Sobirà ;
 Ermengarde, mariée à Guillaume de Castelbon.

Il épouse en secondes noces, en 1006 ou 1007, Toda, comtesse de Ribagorce, mais cette union reste sans descendance.

Notes et références

Voir aussi

Bibliographie

Articles connexes

 Comté de Pallars
 Comtés catalans

Lien externe
 « Sunyer I de Pallars », Gran Enciclopèdia Catalana, consulté le .

Comte de Pallars
Comte de Ribagorce
Histoire de la Catalogne
Noble des Espagnes médiévales


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text:
#include "mlir/Dialect/StandardOps/Ops.h"
#include "mlir/IR/AffineExpr.h"
#include "mlir/IR/AffineMap.h"
#include "mlir/IR/Attributes.h"
#include "mlir/IR/PatternMatch.h"
#include "mlir/IR/StandardTypes.h"
#include "mlir/Pass/Pass.h"
#include "mlir/Support/Functional.h"
#include "mlir/Support/LLVM.h"
#include "absl/memory/memory.h"
#include "llvm/ADT/STLExtras.h"
#include "llvm/ADT/StringSwitch.h"
#include "mlir/Dialect/QuantOps/FakeQuantSupport.h"  // TF:llvm-project
#include "mlir/Dialect/QuantOps/QuantOps.h"  // TF:llvm-project
#include "mlir/IR/Location.h"  // TF:llvm-project
#include "tensorflow/compiler/mlir/lite/ir/tfl_ops.h"
#include "tensorflow/compiler/mlir/lite/quantization/quantization_utils.h"

//===----------------------------------------------------------------------===//
// The Pass to add default quantization parameters for the activations which
// don't have quantization information. These default parameters are usually
// not from real measurement, so this pass is only for test purpose.

namespace mlir {
namespace TFL {
// Includs an auto-generated function, which can retrieve the quantization
// specification for an TFL operation. The signature of the function is
//   std::unique_pointer<OpQuantSpec> TFL::GetOpQuantSpec(Operation *)
#include "tensorflow/compiler/mlir/lite/utils/generated_op_quant_spec_getters.inc"

namespace {
class DefaultQuantParamsPass : public FunctionPass<DefaultQuantParamsPass> {
 public:
  explicit DefaultQuantParamsPass(double default_min, double default_max)
      : default_min_(default_min), default_max_(default_max) {}

  void runOnFunction() override;

 private:
  // Whether the value is used as a bias input of another op. Here we assume
  // bias is used immediately by the user. This assumption is always correct
  // after constant folding.
  bool UsedAsBias(Value value) {
    for (auto &use : value.getUses()) {
      auto biases = TFL::GetOpQuantSpec(use.getOwner())->biases_params;
      if (biases.find(use.getOperandNumber()) != biases.end()) return true;
    }
    return false;
  }

  // Uses `quant_params` to quantize `value` and inserting a pair of
  // tfl.quantize and tfl.dequantize ops for this `value`.
  void QuantizeValue(OpBuilder builder, Value value,
                     quant::QuantParams quant_params);

  // If the value hasn't been quantized, the functions adds it to `values`.
  void AddToWorkListIfUnquantized(Value value, std::vector<Value> *values);

  // Converts the default min/max to the default quantization parameters.
  quant::QuantParams GetDefaultQuantParams(Builder builder);

  // Gets the quantization parameters for the bias of an operation by using the
  // quantization parameters from the non-biases operands.
  quant::QuantParams GetQuantParamsForBias(Operation *op, int bias,
                                           const std::vector<int> &non_biases,
                                           quant::AccumulatorScaleFunc func);

  double default_min_;
  double default_max_;
  quant::QuantParams default_quant_params_;
};
}  // namespace

void DefaultQuantParamsPass::runOnFunction() {
  FuncOp func = getFunction();
  OpBuilder builder(func);

  std::vector<Value> activation_values;
  std::vector<Value> bias_values;

  // First of all, collect all the values (block arguments and op results) which
  // are required to be quantized.
  for (auto arg : func.getBody().begin()->getArguments()) {
    if (UsedAsBias(arg)) {
      AddToWorkListIfUnquantized(arg, &bias_values);
    } else {
      AddToWorkListIfUnquantized(arg, &activation_values);
    }
  }

  func.walk([&](Operation *op) {
    if (op->isKnownTerminator() ||
        op->hasTrait<OpTrait::quant::NoQuantizableResult>() ||
        llvm::isa<quant::QuantizeCastOp>(op) ||
        llvm::isa<quant::DequantizeCastOp>(op))
      return;

    for (auto res : op->getResults()) {
      if (UsedAsBias(res)) {
        AddToWorkListIfUnquantized(res, &bias_values);
      } else {
        AddToWorkListIfUnquantized(res, &activation_values);
      }
    }
  });

  // Apply the default quantization parameters for these activation values.
  quant::QuantParams default_params = GetDefaultQuantParams(builder);
  for (Value value : activation_values) {
    QuantizeValue(builder, value, default_params);
  }

  // Since all the non-biases operands have quantization parameters now, we
  // should be able to propagate them to the bias operand.
  for (Value bias : bias_values) {
    Operation *op = *bias.user_begin();
    auto spec = TFL::GetOpQuantSpec(op);
    for (auto &it : spec->biases_params) {
      quant::QuantParams bias_params = GetQuantParamsForBias(
          op, it.first, it.second.first, it.second.second);
      if (!bias_params) continue;
      QuantizeValue(builder, bias, bias_params);
    }
  }
}

void DefaultQuantParamsPass::AddToWorkListIfUnquantized(
    Value value, std::vector<Value> *values) {
  // If the result isn't with float type, this result is an integer tensor and
  // doesn't require quantization.
  auto tensor_type = value.getType().dyn_cast<TensorType>();
  if (!tensor_type) {
    // There are none type values.
    return;
  }
  if (!tensor_type.getElementType().isF32()) return;

  // If the result is consumed by a quantize op, it has been quantized.
  if (value.hasOneUse() &&
      llvm::isa<TFL::QuantizeOp>(*value.getUsers().begin()))
    return;

  // Add this result to the list to apply the default value.
  values->push_back(value);
}

void DefaultQuantParamsPass::QuantizeValue(OpBuilder builder, Value value,
                                           quant::QuantParams quant_params) {
  Type expressed_type = value.getType();
  Type new_type = quant_params.castFromExpressedType(expressed_type);
  // This value isn't an expressed type (float), skip.
  if (!new_type) return;

  Block &block = value.getParentRegion()->front();
  Operation *op = value.getDefiningOp();
  if (op) {
    builder.setInsertionPoint(&block, ++Block::iterator(op));
  } else {
    builder.setInsertionPointToStart(&block);
  }
  TypeAttr type_attr = TypeAttr::get(new_type);
  auto quantize = builder.create<TFL::QuantizeOp>(value.getLoc(), new_type,
                                                  value, type_attr);
  auto dequantize = builder.create<TFL::DequantizeOp>(
      value.getLoc(), expressed_type, quantize.output());
  value.replaceAllUsesWith(dequantize);

  // `quantize` is using `dequantize` now, so we should set its operand to
  // `value`.
  quantize.getOperation()->replaceUsesOfWith(dequantize, value);
}

quant::QuantParams DefaultQuantParamsPass::GetQuantParamsForBias(
    Operation *op, int bias, const std::vector<int> &non_biases,
    quant::AccumulatorScaleFunc func) {
  std::vector<quant::QuantizedType> non_bias_types;
  non_bias_types.reserve(non_biases.size());
  for (int non_bias : non_biases) {
    Operation *non_bias_define = op->getOperand(non_bias).getDefiningOp();
    if (auto dequant = llvm::dyn_cast<TFL::DequantizeOp>(non_bias_define)) {
      auto non_bias_type = dequant.input().getType().cast<TensorType>();
      auto non_bias_ele_type =
          non_bias_type.getElementType().cast<quant::QuantizedType>();
      non_bias_types.push_back(non_bias_ele_type);
    } else {
      // The non-bias hasn't been quantized, let's skip this bias.
      break;
    }
  }
  // The non-bias hasn't been quantized, let's skip this bias.
  if (non_bias_types.size() != non_biases.size()) return {};

  return func(non_bias_types);
}

quant::QuantParams DefaultQuantParamsPass::GetDefaultQuantParams(
    Builder builder) {
  if (!default_quant_params_) {
    default_quant_params_ = quant::fakeQuantAttrsToType(
        builder.getUnknownLoc(),
        /*numBits=*/8, default_min_, default_max_, /*narrowRange=*/false,
        builder.getF32Type());
  }
  return default_quant_params_;
}

// Creates an instance of the default quant parameters pass.
std::unique_ptr<OpPassBase<FuncOp>> CreateDefaultQuantParamsPass(
    double default_min, double default_max) {
  return absl::make_unique<DefaultQuantParamsPass>(default_min, default_max);
}

// Registers this pass with default values, only for test
static PassRegistration<DefaultQuantParamsPass> pass(
    "tfl-default-quant",
    "Apply quantization with default quantization parameter", [] {
      return CreateDefaultQuantParamsPass(/*default_min=*/-1.0,
                                          /*default_max=*/1.0);
    });

}  // namespace TFL
}  // namespace mlir

redpajama_set_name: RedPajamaGithub


text:
Pierre Tribié est un syndicaliste français

Biographie
Né le  à Puteaux (Seine), il devient tour à tour auxiliaire de perception (1926) .  ,  inspecteur du trésor (1945), receveur-percepteur des finances (1968), trésorier principal des finances (1971) puis trésorier principal honoraire (1971-1978).

De 1944 à 1947, il est permanent de l'Union départementale CGT de la Seine, en service détaché et payé par le syndicat. Secrétaire général de la Fédération des Finances Force ouvrière en 1952 et 1953 il devient secrétaire général de la Fédération générale des fonctionnaires - Force ouvrière (FGF FO) de 1953 à 1973.
De 1954 à 1977, il est trésorier de la confédération Force ouvrière

Administrateur de la Société générale (1951-1980), membre de la Commission des comptes et des budgets économiques de la nation (1959-1971), membre du Conseil économique et social représentant les organisations syndicales CGT-FO (1959-1974), membre du conseil d'administration de l'Ecole nationale d'administration (1964-1971), de l'Erap (1969-1982), il est nommé en juin 1971 conseiller d'Etat en service extraordinaire (1971-1975).

Il est mort le  à Sartrouville (Yvelines).

Notes et références

Syndicaliste de Force ouvrière
Naissance en juillet 1910
Naissance à Puteaux
Décès en mai 2002
Décès à Sartrouville
Décès à 91 ans
Naissance dans le département de la Seine


text:
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Foreign Relations of the United States, 1952-1954, Iran, 1951–1954, Second Edition
Document 115
115. Memorandum From the Director of the U.S. Technical Cooperation Administration Mission in Iran (Warne) to the Ambassador to Iran (Henderson)1
Tehran, August 12, 1952.
My visit with Seyed Abdol Ayatollah Kashani
At his request brought to me by one of his sons and after discussing the matter with you, I went to a home in Shimron at 11 a.m. on August 11 to meet Ayatollah Kashani. Present at most of the conference also was Mr. Shams Ghanat-Abadi, a mullah, reported son-in-law, and close follower of Kashani, who is a deputy from Shahrod, and two sons of Kashani, one a mullah named Khashanizahed Kashani, and the other named Mostafa Kashani.
After waiting some 30 minutes while Kashani completed a conference with mullahs in another room, I was joined by Ayatollah Kashani. He appeared most interested in our conference; to the point indeed of keeping me there past 1 o'clock, which is his lunch time, through luncheon, and until his siesta period at 2 p.m. The conference, of course, was slower than those we might hold where only one language is spoken because of the necessity of translating carefully everything that was said. I was accompanied by Mr. Ardeshir Zahedi, of Point 4, who acted as interpreter for the conference.
At the outset, I congratulated Kashani on his election as President of the Majlis. I said this was a great honor but also a great responsibility in these times. He replied that he considered it as a very small matter since long before he had been spiritual leader of most of the Middle East. I said I recognized the responsibilities he had carried as spiritual leader of millions but I did not think one could over-emphasize the importance of being President of the Majlis in Iran at a time when Iran held such a fateful position in the world. He then said that his position as spiritual leader gave him great power as the events of last month had clearly shown. He said he would give his life for his country and was motivated only by its best interests. He said when Great Britain and the United States brought in Qavam as Prime Minister his displeasure was based on the fact that it was not in the interests of Iran and his displeasure was reflected in the demonstrations that overthrew Qavam. He said some people thought the communists had joined him but he assured me that he was even more against the communists.
[Page 318]
Kashani said long ago he was visited by a Mr. Dooher who asked his help in bringing Razmara to power. He said he told Mr. Dooher the United States would be making a mistake to bring Razmara forward and this had proved to be so. He said that 20 days before Qavam came in he had evidence of Anglo-American joint action to that end and that such action had been a mistake, too.
At this point I said it was not true that the United States had assisted in bringing Qavam into power and that I could assure him that the United States did not interfere in the internal affairs of Iran. I said we had no advance information of Qavam's coming to power. I said, however, if he wanted to discuss political and diplomatic questions they should be brought up with you, the United States Ambassador, and these were not my field of responsibility.
When this was translated to Kashani, he dropped the subject (a little to my surprise) and political matters were not again discussed. The conference turned completely to a discussion of the Point 4 program and plans for the economic development of Iran. Several things stand out as very pointed impressions of this conference. These are:
(1) Ayatollah Kashani, though elderly, is vigorous and alert.
(2) Ayatollah Kashani seems to be isolated. He is surrounded by his own relatives and a few mullahs, and almost no one else seems to be on intimate terms with him.
(3) Ayatollah Kashani has sublime faith in his religious leadership. He believes that this gives him extraordinary power of leadership in Iran. I believe that he has no doubt that he could rally the people for or against almost any other institution or influence.
(4) Ayatollah Kashani and his intimate followers have little conception of what goes on outside relatively narrow circles. They know little of the Western world or of the Eastern world outside their homeland.
(5) Ayatollah Kashani does not seem to be an unfriendly person or lacking in warmth and seems to have an underlying compassion for the poor peoples of Iran.
As we talked, Ayatollah Kashani said he hoped that Point 4, the programs of which I had carefully explained to him from A to Z, would do something "Really substantial" for Iran. He thought a big dam in the river near Isfahan and a dam on the Karun would be good ideas and would meet his specifications. He asked me how much I thought such dams would cost. I told him I could give him only the barest horseback opinion but through familiarity with the work of the Bureau of Reclamation of the United States, in which I had served for many years, and as a result of a fairly good reconnaissance of the Karun River made earlier this year, I thought 200 to 250 million dollars would be required to [Page 319] develop a satisfactory project on the Karun involving storage of water, generation of electric power, irrigation by pumps and by direct diversion, and the possibility of navigation on the lower river and through large canals to Bandarshapur. He appeared amazed and said he thought 100 dams could be built for 200 million dollars. I said one could not generalize about the cost for dams but that good engineering work had to precede the design and construction of any such project to provide sound estimates. I said I knew costs in the United States, however, and big dams cost big money anywhere.
Ayatollah Kashani again urged me to advocate "substantial work" by the United States in Iran and suggested that I should go to the United States immediately to present the case for such works. I told him that I was in agreement as to the need for projects to develop and utilize resources of Iran and that I had given a great deal of thought to such projects. I said that Point 4 had directed a part of its work into those areas and that I thought we might be able to bring forward specific designs and specifications of projects that could be adopted by the International Bank or Export-Import Bank or some other agency that might provide the necessary capital. I said it seemed to me that Iran would need a stable flow of foreign exchange before such works could be prosecuted which indicated the need for a settlement of the oil issue and a resumption of oil sales.
I said that Point 4 would be very happy to work with the Iranian Government agencies in attempting to prepare substantial programs for internal improvements in Iran though I doubted that the present program would be able to finance the large capital requirements of any such improvements. I asked whether he or Mr. Ghanat-Abadi had suggestions as to programs that might be taken up. I said that I thought responsible leaders of the government ought to assist in the development of plans. No other suggestion than the two dams mentioned above were made. Instead I was asked for some suggestions.
I mentioned the discovery of oil at Qum and the possibility of developing a project for low cost kerosene as a substitute fuel in the rural areas. This seemed to interest and excite them. They said if I could not go to the United States to present the requirements of Iran for substantial development they hoped I would write. I said I had been reporting the needs of the country and would try to continue to do so.
Throughout the conference reference to communist activities and the threat of communism were made by Mr. Kashani and Mr. Ghanat-Abadi. They always spoke of the communist activities as something deleterious to the country and antagonistic to their positions.
At one point Ayatollah Kashani said the misery of the people alone could turn them away from their faith and to communism. He said he did not fear his ability to rally the people to patriotic action unless the [Page 320] people became more desperately hungry when he feared they would turn to communism. The notes of my interpreter at this point contain "Mr. Kashani added that communism was the worst enemy of Iran and that to stop communism the present deplorable condition of the people should be improved. A hungry person will not go after moral values and religion."
At another point Mr. Kashani referred to his dislike of the British and his equal dislike of the Russians. He said he would like to see the friendship between Iran and the United States strengthened in order that Iran might be better able to resist communism.
I said that our program was not "anti-communistic" but was a constructive program to help Iran help herself. I said I did not wake up each morning thinking, "How can I fight communism?" but I woke up each morning thinking, "How can I assist in fighting the diseases, hunger, and poverty that plague the people of Iran?" I said that if this was an attack on the roots of communism then communism was a diseased plant and ought to be rooted out.
Kashani said he was devoted to the welfare of the people, and he thought substantial programs of improvement were needed because the people were sick and hungry.
One time when Mr. Kashani mentioned substantial programs he said something that deprecated a bit the Point 4 deep water well program. Mr. Ghanat-Abadi interrupted him and said "do not under estimate the well program. Do not say anything against it. I need a Point 4 well at Shahrod or I may not be reelected."
Unlike many Iranians, Kashani had no pet or personal projects to put forward. The only time he mentioned a specific project for our consideration was in connection with a discussion of the plight of some of the poor people south of Tehran. He said some of these people, perhaps communist-led, had been squatting on land belonging to the government or others. He said he thought it would be appropriate for Point 4 to consider putting in a couple of wells to serve these people since they were needy and their lot was indeed hard. He thought that might keep them from desperate actions.
Near the close of the conference, Mr. Kashani said he appreciated the efforts of Point 4 to assist Iran but he wanted me to inform my countrymen of the conditions and needs of this country. He expressed his hope for the success of this American mission "Inshallah"—God willing.
Before the conference closed, Mr. Ghanat-Abadi asked permission to take up a matter or two with me. He said that some people had come to him and attacked Point 4 on the grounds that we did all our trucking business with Levant Express which was run by Armenians. He said that he did not mean that we should avoid Armenians because of reli[Page 321]gious differences with the Moslems but that we should take into consideration that as a minority group they have for centuries acted as spies against the country and they welcomed the Russians with wreaths and they welcomed the British with wreaths. He thought Iranian enterprises should not be rejected in favor of Armenians. I said I hoped he understood that religious and racial differences were not taken into consideration in public matters in the United States and that our government attempted to maintain consistent policy of non-discrimination and that I was trying to do the same in the work of Point 4 here. I said that whenever anyone could show that he could do our transportation business cheaper and better than Levant he would get the business. I said, further, that we had endeavored to maintain a local employment policy that would keep Moslems and Armenians at the relative proportion in our organization that they had throughout the country.
After the luncheon for which I had no previous intention to stay but to which I was urgently and repeatedly invited, I made my adieus and left with the thanks of Mr. Kashani for a pleasant conference and his expressed hope again for the success of the mission. As I left, he again mentioned the need of the people of Javadeyeh, which is close to the railroad station south of Tehran, for drinking water.
William E. Warne2
Source: National Archives, RG 469, Records of U.S. Foreign Assistance Agencies 1948–1961, Mission to Iran, Executive Office Subject Files (Central Files) 1951–1961, Box 6, Folder 7, Travel Development—Political 1952. Confidential.↩
Printed from a copy that bears this typed signature with an indication that Warne signed the original.↩
Iran, 1951–1954, Second Edition
Abbreviations and Terms
Foreign Relations, 1952–1954, Iran, 1951–1954 (Documents 1-375)
The July 1952 Iranian Political Crisis and Its Aftermath, March 1952–February 1953 (Documents 67-168)
Qavam Es Sultaneh, AhmedDooher, Gerald F.P.Henderson, Loy W.Kashani, Seyed Ayatollah Abdol GhassemRazmara, Lieutenant General Haji AliWarne, William E.Zahedi, Ardeshir
Abbreviations & Terms
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Guide to sources on Vietnam, 1969-1975
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In a world filled with crazy colors, superfluous synthetics, and brash brands, there is none more in touch with their "wild side," than Puma. However, it seems that, at least for their latest release, Puma has decided to take a step away from all the modern mayhem that we associate with soccer cleats, and deliver something that boasts quality derived from years gone by. The Naturale Puma King "Made In Italy": a pair of boots that don't need any frills associated with modern tech, uppers, or soleplates. It's "Old School" in the best way possible…I'm afraid we'll need a dozen or so…for a friend.
For the two particular sensibilities, Puma has given this boot two fantastic color options. For the purist, a deep, golden brown option with red trim. A beautiful boot that absolutely screams about the history that this boot has seen, and something that would look totally perfect sitting on a mantle or getting stuck into a challenge. The other colorway is a clean white leather, with neon yellow trimmings. The yellow does hint towards more modern leanings, but it simply allows the boot to glow and bask in its own brilliance.
Puma might be the first brand to head towards "weird," but this collection is pure and simple perfection. We might be heading into brave new worlds with the boots that 2016 has seen, but these boots will never find themselves without an appreciative fan-base. Timeless, and a big win for the big cat. Hurry up and join the land of the kings, before these find themselves stuck in the pages of history.


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UK Constitutional Reform Tracker
Constitutional developments and the central government
About the tracker
Using the tracker
We are living in constitutionally eventful times but constitutional reform is not being approached in a unified way under a single Bill, review, or commission. Instead, policies which have constitutional implications are being pursued at different times by different departments in different ways to achieve different objectives. Moreover, much of the change produced may not even be intentional. It is the unexpected consequence of a series of measures taken together.
This makes it difficult to keep track of what is going on, in which department, why it is important, how it interrelates with other changes, and what its broader or longer-term implications might be. Public Law Project's UK constitutional reform tracker tries to tackle this problem.
How does the tracker help?
The tracker does two important things. The first is to provide a chronological list of constitutionally important events under the current administration. Given that the current constitutional reform trend is not exclusively or even largely legislative in some areas, these important events include not only primary legislation but also secondary or delegated legislation issued by Ministers, policy papers, parliamentary motions, ministerial statements, government speeches and announcements, public appointments, administrative practices, and key cases from the courts associated with these things. The purpose is to highlight events that may otherwise be obscure or missed.
The second important feature of Public Law Project's tracker is to make every one of these entries searchable by various tags. This will help users understand not only what is going on in terms of individual changes but also the interrelationships between events, so that trends and patterns over time can be seen. Users can search, for example, for all policies that have implications for judicial review, or freedom of expression, or national security, or which relate to the ministerial code. Users can also search for activities related to particular central government departments or institutions and several other categories and themes, available here.
Scope and nature of the tracker
Importantly, the tracker is designed to be politically neutral and impartial. We make no assessment of whether the events it contains are good or bad. Instead, the tracker is designed to be a shared resource for those interested in constitutional issues without addressing political debates as to the merits of each proposal or event. Those are assessments we prefer to leave to the users of the tracker.
The tracker focuses on events of constitutional relevance and significance pursued by the central government and the immediate consequences of those reforms, such as court cases, comments by the Speaker of the House of Commons, and parliamentary reports. It does not, at this stage, focus on independent constitutional reforms pursued by the devolved governments or other bodies.
UK Constitutional Reform Tracker, Blog at WordPress.com.


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Lamar Odom Says He Deeply Regrets Cheating on Khloe Kardashian
HOLLYWOOD - SEPTEMBER 21: Television personality Khloe Kardashian (L) and Los Angeles Laker Lamar Odom attend the "AXE Music One Night Only" concert series featuring Weezer at Dunes Inn Motel - Sunset on September 21, 2010 in Hollywood, California. (Photo by Michael Buckner/Getty Images For AXE)
Beasley Media Group Editoral	May 15th
CENTURY CITY, CA – MAY 18: NBA player Lamar Odom and TV personality Khloe Kardashian arrive at the 19th Annual Race to Erase MS held at the Hyatt Regency Century Plaza on May 18, 2012 in Century City, California. (Photo by Frazer Harrison/Getty Images for Race to Erase MS)
Lamar Odom is opening up about his very public divorce from ex-wife Khloe Kardashian and his decision to be unfaithful to the reality star.
In his upcoming memoir, Darkness to Light, Odom reveals that he has deep regrets about the end of his four-year marriage to Kardashian and the way he treated her.
In an interview with People Magazine, who previewed the memoir exclusively, he gets candid about his choices.
"I wish I could have been more of a man," Odom says. "It still bothers me to this day. But regret is something we have to learn to live with."
The former NBA star also revealed that he hid a longtime addiction to cocaine from his wife.
"At the start of our marriage I was faithful to her," he said, before revealing that he succumbed to his demons and gave into cheating and drug addiction.
"I could not handle the lethal cocktail of the spotlight, addiction, a diminishing career and infidelity," he writes. "Oh, did I mention the paranoia, anxiety, depression. … I couldn't keep my d— in my pants or the coke out of my nose. Drug addicts are incredibly skilled at hiding their habit. I'd get defensive and Khloé would just drop it."
Eventually, Kardashian found out about his infidelity and the couple split. But when Odom overdosed and nearly died, Kardashian stayed by his side and helped nurse him back to health.
"Her love for me must have been unconditional," he said. "That's the only thing [I think] that gave her the strength to still love me at that time."
Odom is now clean and sober and revealed that he hopes he can be friends with his ex-wife again.
"I hope we can be friends," Odom says. "I miss the family. And I hope we can all be reacquainted one day."
His memoir, Darkness to Light, is out May 28.
KVGS
Khloe Kardashian,Lamar Odom
2019 Regal Summer Movie Express!
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Say goodbye to last minute hassles at the airport with our Pre Paid Baggage Allowance Scheme.
Excess baggage is the additional weight you intend to carry beyond the permitted Free Baggage Allowance.
The scheme covers all Air India's international flights.
The scheme has four slabs for routes on which weight concept is used to charge for excess baggage. Each slab will have a uniform discount rate of 20%. A passenger can call the call centre or go to the Air India booking office and purchase for himself a baggage allowance in return for payment. E.g. one can make a payment and purchase a baggage allowance with a maximum limit of 5 Kgs for economy class. Now the passenger can travel with an excess baggage going up to a maximum of 5 Kgs without going through the process of making the payment at the airport. Also, by purchasing through the call centre or Air India booking office he will be paying 20% less than he would have paid at the airport. Passenger will not get any refund for any unutilized excess baggage. In the example even if he carries 3 Kgs excess baggage, he will not be refunded for the unutilized 2 Kgs.
Routes where piece concept is applicable, 20% discount will be given on both extra piece and excess weight on the free baggage piece i.e. excess weight above 23Kgs and up to 32Kgs.
This scheme also covers Domestic flights.The scheme has five slabs which has 20% Discount upto 25Kgs.
One passenger is allowed to purchase pre-paid baggage allowance of maximum 25Kgs on Domestic Flights and maximum 20Kgs on International flights. Any excess weight over and above the mentioned weights has to be paid as per normal excess baggage rate applicable at the Airport.
International Routes where "Piece Concept" is used, a passenger can avail maximum of 2 additional pieces under this pre-paid baggage scheme.
Excess baggage cannot be purchased through call centre or booking office (CTOs) within (6 hours) hours of departure of the flight on which the passenger is planning to travel.
Excess baggage is not applicable for Multicity travel, unless the Passenger is in Transit and the Baggage is "Through Checked-in".
In case the booking is cancelled as per the fare terms, amount for excess baggage purchased through call centre or booking office (CTOs) will be refunded in full.
Passenger may cancel his/her pre-paid baggage allowance up to 6 hours prior to scheduled or revised departure, as the case may be, for flights operated by Air India.
Excess baggage purchased through call centre or booking office (CTOs) is non-endorsable, non-transferable and not applicable for infant.
No part or full refund will be permitted at the check-in counter, for baggage weighing lower than the purchased excess baggage limit. I.e. amount for unutilized excess baggage weight cannot be refunded or used on subsequent flights.
Refund on excess baggage purchased will be applicable:(i) If the passenger chooses to cancel the flight booking 6 hours before departure or(ii) If Air India cancels the flight.
Purchase of excess baggage through call centre or booking office (CTOs) is applicable for passengers holding a valid e-ticket having ticket number commencing with 098 series.
Purchase of excess baggage through call centre or booking office (CTOs) is not permitted for Alliance Air, Air India Express and Air India's code share and interline flights. It is permitted only on Air India flights on any of its domestic and international routes operated exclusively by Air India flights with Air India flight numbers.
In case of 'No Show', excess baggage purchased will not be refunded.
Excess baggage purchased must be utilized by the passenger for the flight booked and for checked-in baggage only.
In case a passenger is holding a return, ticket and wants to purchase pre paid excess baggage for both the segments in his PNR/ticket, he will be required to make two separate payments.


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Garcia Live Volume Nine is a two-CD live album by Jerry Garcia and Merl Saunders.  It was recorded on August 11, 1974 at the Keystone in Berkeley, California.  It was released on July 28, 2017.

The musical lineup for this concert was Garcia on guitar and vocals, Saunders on keyboards and vocals, Martin Fierro on saxophone and flute, John Kahn on bass, and Bill Kreutzmann on drums.  A slightly later version of this band, with a different drummer, was called Legion of Mary.

Critical reception
On AllMusic, Timothy Monger wrote, "Captured in the period between the release of the Grateful Dead's From the Mars Hotel LP and their touring hiatus that began in late 1974, this lively set from Jerry Garcia and longtime collaborator Merl Saunders has a comfortable, spontaneous ease to it....  By this point, the Saunders-Garcia partnership was already well established and their preferred venue, Keystone Berkeley, provided a relaxed space to try out the various facets of their funk, rock, and R&B repertoire.... The highlights, though, are in the extended jams, particularly the 19-minute "The Harder They Come", which feels like a dynamic zenith of this set."

On Grateful Web, Dylan Muhlberg said, "GarciaLive Volume Nine: August 11, 1974, Keystone Berkeley is like nothing you've heard previously from the Jerry Garcia catalog. It's remarkable how the supple drumming of Bill Kreutzmann varies the groove entirely, compared to Garcia's previous collaborator Bill Vitt and future associate Ron Tutt... Fans of Jerry Garcia need to get their hands on this release... This is like nothing you've ever heard before, with crystal-clear transfer. You'll be taken from your living room back to the intimate confines of the Keystone, Berkeley, for a night of infinite possibilities."

On Glide Magazine, Doug Collette wrote, "The nine selections of Volume Nine in this archival series well illustrate how a setlist can oftentimes barely scratch the surface of what went on below and beyond the songs documented in a given night's performance.... Precursor to the band eventually dubbed Legion of Mary that coalesced later this same year, this quintet displays the same predilection to dig deeply into a groove, the depth of which recordist Betty Cantor-Jackson captures with her usual impeccable clarity (and which Fred Kevorkian preserves with his equally reliable mastering)."

Track listing
Disc 1
First set:
"That's What Love Will Make You Do" (Henderson Thigpen, James Banks, Eddy Marion) – 13:14
"La La" (Martin Fierro) – 17:06
"It Ain't No Use" (Jerry Williams, Gary Bonds, Don Hollinger) – 10:57
"Mystery Train" (Junior Parker, Sam Phillips) – 13:33

Disc 2
Second set:
"The Harder They Come" (Jimmy Cliff) – 19:10
"Ain't No Woman (Like the One I've Got)" (Dennis Lambert, Brian Potter) – 17:01
"It's Too Late" (Chuck Willis) – 9:06
"(I'm a) Road Runner" (Brian Holland, Lamont Dozier, Eddie Holland) – 10:43
"The Night They Drove Old Dixie Down" (Robbie Robertson) – 6:34

Personnel
Musicians
Jerry Garcia – guitar, vocals
Merl Saunders – keyboards, vocals
Martin Fierro – flute, saxophone
John Kahn – bass
Bill Kreutzmann – drums

Production
Produced by: Marc Allan, Kevin Monty
Original recordings produced by: Jerry Garcia
Recording: Betty Cantor-Jackson
Mastering: Fred Kevorkian
Art direction, design, illustration: Ryan Corey
Liner notes essay: Merl Saunders, Jr.
Photos: Larry Hulst, Roberto Rabanne
Project coordination: Lauren Goetzinger

References

Jerry Garcia live albums
Merl Saunders albums
2017 live albums