text:
\section{Introduction}

As observational instruments have developed,  systematic studies of
stellar clusters have revealed
many low-mass populations of pre-main sequence (PMS) stars in massive star-forming regions.
It has been found that most stars are born in groups or clusters, not in isolated regions \citep[e.g.,][]{lad03, all07}.
Stellar clusters
provide a tool for investigating stellar evolution, because
they are considered to constitute a natural sample of coeval stars at the same distance
and with the same chemical composition.
Young clusters appear to be  a snapshot of stellar evolution over a wide range of masses.
However,
a careful study of the Orion Nebula Cluster \citep{hil97}  has revealed
that the younger stars ( $<$ 0.3 Myr )  are clustered towards the center of the Trapezium Cluster
(a projected distance of $<$ 0.3 pc from ${\theta}^1$C Ori), while the older stars are widely distributed.
This indicates that star formation has recently occurred in the center of the cluster and that star formation
with a low rate has taken place over a long time scale over the whole region.
\citet{mue08} has suggested that there is no physical reason to
separate the Orion Nebula Cluster and the Trapezium Cluster, and the entire
region is a single contiguous star forming event.
There are also examples of stellar clusters still producing massive stars.
Cep A HW2 is the brightest radio source in Cep A \citep{huw84},
an active star forming region within the molecular cloud associated with the cluster
with an age of 5.5 Myr \citep[Cep OB3b;][]{jor96}.
\citet{Jim07} found a hot core internally heated by a massive protostar,
and a circumstellar rotating disk around HW2.
This suggests that a massive star is still forming in the young cluster.
Furthermore, X-ray stars with a mid-infrared (MIR)  spectral energy distribution of
young stellar objects (YSOs) around HW2 have been reported by \citet{prv09}.
It is most likely that a low-mass PMS population was already formed before the formation of high-mass stars.
Once a high-mass star starts to radiate significant amounts of UV radiation,
the surrounding material is affected dramatically and the natal molecular cloud is disrupted
and the birth of the next generation of stars might be triggered.

The apparent age spread observed in the color-magnitude diagram of young stellar
groups has been investigated by \cite{bur05}.
They found that the spread could not be explained adequately by the combination of the binarity,
photometric uncertainty and variability of the members.
In the case of the $\sigma$ Ori young stellar group,
they suggested an age spread of 2--4 Myr.
A possible explanation is that accretion from a disk causes
scatter of the stellar continuum light \citep{tou99}.
However, another possibility is that  stars in a cluster are
formed over a period of time.
Three-dimensional numerical simulations including protostellar outflow feedback
show that the cluster-forming clumps can maintain a quasi-virial equilibrium state
for several periods of free-fall time \citep{nal07}, suggesting continuous star formation.
\citet{wan10}  also demonstrated  outflow-regulated massive star formation.
The episodic star formation causes an intrinsic spread in age and hence in the position in the color-magnitude diagram.

We have reported that young stars near the exciting star of the W5E H {\sc ii} region are
systematically older than those near the edge of the H {\sc ii} region  \citep{nak08}.
We further suggested that the birth of the most massive star occurs in the late stage of star formation in the cluster.
Although the structure of the H {\sc ii} region is simple to investigate, the distance of W5 is large, at 2.3 kpc,
and therefore it is not easily accessible
to the wide range of stellar masses.

IC 1396 is a ring-shaped giant H {\sc ii} region in Cep OB2 with a size of about 3$\degr$,
located at the edge of the Cepheus bubble, which is a large, far-infrared shell with a diameter
of $\sim$10$\degr$ \citep{kun08}.
The structure of  IC 1396 is rather simple and is powered by the
multiple O star system HD 206267 (RA = 21$^h$38$^m$57$\fs$62, Dec = +57$\arcdeg$29$\arcmin$20$\farcs$5), which is located near the
geometrical center of IC 1396  in the young cluster Trumpler 37.
The bright members of Trumpler 37 have been investigated by many authors \citep[e.g.,][]{gar76, mar90, dez99, con02}.
There are a number of bright-rimmed globules \citep{pot56} at its periphery.
Its modest distance ($<$ 1 kpc) and low foreground extinction ($A$v $<$ 1 mag) make IC 1396 a good subject for
our study of low-mass population associated with OB stars.
The mean distance of 76 members of Cep OB2 derived from the Hipparcos parallax is 615 pc  \citep{dez99}.
\citet{con02} made a color-magnitude diagram of the intermediate-mass members and fitted them to
main-sequence stars at 870 pc.
In this paper, we adopt 870 pc, which is frequently quoted by the recent works  \citep[e.g.,][]{sic04} .

H$\alpha$ emission, a characteristic of T Tauri stars (TTS), is radiated from the solar-type
magnetic activity in weak-lined T Tauri Stars (WTTS) or the chromospheric activity and magnetospheric accretion shock in
classical T Tauri stars (CTTS)  \citep{bri07}.
Thus, a survey of H$\alpha$ emission-line stars is a powerful method for searching
for young low-mass populations \citep[e.g.,][]{nak95}.
Recently, NIR observations with  array detectors and
MIR observations from space (e.g. with  the {\it Spitzer} Space Telescope) have advanced
the protostar survey in the dense parts of giant molecular clouds.
However, the H$\alpha$ survey is still useful in areas with moderate or low extinction, and it is also a complementary
method to search for PMS populations in a wide and rather dispersed region.
Here, we report an extensive survey of emission-line stars in the IC 1396 H {\sc ii} region and discuss
the formation sequence of low and high mass populations in IC 1396.

\section{Observations}

Slitless grism spectroscopic searches for H$\alpha$ emission objects in IC 1396 were conducted
in 2004 and between 2006 and 2009 using the Wide Field Grism
Spectrograph 2  \citep[WFGS2; ][]{ueh04} at the f/10 Cassegrain focus of the
University of Hawaii (UH) 2.2-m telescope on Mauna Kea.
The log of the observations is given in Table 1.
A 300-line mm$^{-1}$ grism was used in conjunction with a wide H$\alpha$ filter to isolate
the first-order spectra between 6265--6765 {\AA}.
A Tektronix 2048$\times$2048 CCD was used as the detector, yielding a dispersion of
3.8 {\AA} pixel$^{-1}$, a pixel scale of 0$\farcs$34  and an instrumental field of
view of 11$\farcm$5 $\times$ 11$\farcm$5

The whole IC 1396 region was covered by 157 field positions including overlapping areas.
About 4.2 deg$^2$ were observed, both in the grism and the direct imaging mode of WFGS2.
Figure 1 shows the boundary of the observed fields and indicates the names of bright-rims,  dark clouds,
and two O stars in the IC 1396 H {\sc ii} region.
For each field, we have taken a single 30-s exposure in the direct mode with a wide H$\alpha$ filter.
Then, we inserted a grism and obtained  three dithered frames of 300-s exposures  for
slitless spectroscopy.
Direct images with an $i'$-band filter were also taken with WFGS2 in 2008 August and 2009 August.
Three 30-s exposures were made for each field.
The $i'$-band flux is less affected by  excess emission of the circumstellar disk, H$\alpha$ emission, and
continuum veiling of CTTS.
Thus,  $i'$-band photometry is useful as a measure of the underlying photosphere of CTTS
\citep[e.g.,][]{cie05}.
3--5 standards for the Sloan Digital Sky Survey (SDSS) system \citep{smi02} were observed each
night at nearly the same
airmass (difference of $<$ 0.1) as the targets.   We used a dome flat for flat fielding.

The data were reduced using the IRAF software package.
We applied the standard procedure for bias subtraction and flat fielding.
For each field, three dithered grism frames are combined into one frame by referring the position of
the H$\alpha$ emission or absorption line of the star(s) in the field.
We picked all stars in each wide H$\alpha$ image using the DAOFIND package
and extracted their one-dimensional spectra from the grism
image. We visually investigated the spectra for the presence of the
H$\alpha$ emission line and found 639 H$\alpha$ emission-line objects in the whole surveyed area.
We used the SPLOT package to measure the equivalent width
of the H$\alpha$ line in the spectra.  Their coordinates were determined by the astrometric
calibration tool of the Starlink program {\it GAIA} using  USNO-B  catalog stars as the reference in the field.
All of the photometric measurements were made with the APPHOT package for aperture photometry.
The typical seeing of the image was 2.7--3.0 pixels.
We used  a 4-pixel diameter aperture for the aperture photometry.
We then calibrated the photometric values to the SDSS system via standards.
In general, the run was of high quality, but thin cloud affected a few fields.
We checked the stability of the magnitude for three direct images in each field and examined the quality of the measurement.
Excluding stars with saturated images or images with low photometric quality, we measured 586 stars in 13.6  $<$ $i'$ $<$ 19.3.

\section{Results}

\subsection{Spatial Distribution}

We  list the 639 H$\alpha$ stars in Table 2.
The table shows the (1) identification number, (2, 3) J2000 coordinates, (4) $i'$-band magnitudes and
(5) equivalent widths of H$\alpha$ emission ({\AA}).
The H$\alpha$ equivalent widths were measured for 608 stars.
We compared our list of emission stars with the Two Micron All Sky Survey (2MASS) Point Source Catalog
with 12 stars supplemented by the 2MASS 6x Point Source Catalog.
We found matches for 617 stars with 2MASS stars within 2$\arcsec$ and determined that 548 of these have good quality $JHKs$ photometry (quality flag AAA).
Due to small separation angles or positional uncertainties,
two pairs of  H$\alpha$ stars are identified with single 2MASS sources
(No. 250/251 with J21381703+5739265, and No. 600/601 with J21451578+5717392).
We have included these stars in the above number.
We list the 2MASS designation of the NIR counterpart, photometric quality, $J$ magnitude, and $J$--$H$, $H$--$Ks$ colors
in columns (6)--(10) of Table 2.
$A$v estimated from the NIR color--color diagram (see \S 4.1) is also listed in column (11).
About 70\% of our H$\alpha$ stars cannot be identified with known sources in
the SIMBAD database.
The identification in the literature or comments are listed in column (12).

Figure 2a shows the spatial distribution of emission-line objects
while Figure 2b represents the contour map of the number density of the detected emission-line objects with
the kernel method \citep{gom93}.  We adopted a Gaussian shape for the density distribution
of the kernel with a smoothing parameter of h$=$2$\farcm$4.
The isolines are drawn at intervals of 150 stars per deg$^2$, which is about three times the average number density
in the field region (see Table 4), starting from 100 stars per deg$^2$.
It is clear from Figure 2 that the distribution of emission-line stars is far from uniform.
To demonstrate
the different properties in the different areas, we divided the surveyed field into
the following subregions according to the number density of H$\alpha$ stars.
The primary peak of the most rich aggregate (the West region) is located between the main exciting star
HD 206267 and  the western elephant trunk globule Rim A (IC 1396A).
The secondary peak is at the opposite side, to the east of HD 206267 (the East region),  and
the third peak is at the south of the bright-rimmed globule SFO 38  (SFO: \citealt{sfo91}, the SFO38 region).
Other small aggregates of emission-line stars are located near SFO 37 (the SFO37 region), SFO 39 and SFO 41
(the SFO39/41 region), Rim B (the Rim B region), and at the north of the B 365 dark cloud (B: \citealt{b27})
or around (21$^{h}$35$^{m}$, $+$57$\degr$).  See Figure 1 for references.
The West and the East regions appear to be surrounded by a halo-like structure (the Halo region).
Some H$\alpha$ stars appear to be associated with other small bright rimmed clouds
such as Rim C and SFO 34 (Rim D).
We defined the rest of the region as the field area (the Field region).

\subsection{Source Identification }

Our sample of H$\alpha$ stars  contains  two carbon stars CGCS 5454 (No. 575) and CGCS 5401 (No. 287),
and one Be/X-ray binary Cep X-4 (No. 340), whose distance was confirmed to be 3.8 kpc by \citet{bon98}.
Our sample of H$\alpha$ stars also contains a candidate of the exciting source  of the Herbig--Haro object
HH 588 (No. 436), which is deeply embedded in
SFO 37 \citep{ike08}, one Herbig Ae/Be star (HAeBe) MVA 426 (No. 236) \citep{sic07},  and $\sim$ 100 TTS
including Class-II, III, and transient objects  \citep{sic06b, sic07, get07, rea04, mer09, bar11}.

An objective prism survey using the Schmidt telescope \citet{kun86} detected 155 H$\alpha$ emission objects in IC 1396
and an additional 65 emission stars were reported in a subsequent paper \citep{kup90}.
Their spatial distribution shows no noticeable concentration or clustering.
Out of 220 Kun H$\alpha$ stars, 150 stars are located in our observed field; however,
only 11 stars (No. 287 = Kun 80, No. 13 = Kun 171, No. 340 = Kun 193, No. 618 = Kun 215,
No. 49 = Kun 308, No. 80 = Kun 310, No. 97 = Kun 314 S, No. 252 = Kun 321, No. 318 = Kun 325,
No. 410 = Kun 330, No. 487 = Kun 332) are identified among our H$\alpha$ stars.
Although Kun 315 (LkH$\alpha$ 349) is not included in Table 2, our grism spectrum appears saturated
but indicates a P Cyg-type H$\alpha$ profile.
Kun 320 (GL Cep) and Kun 337 (HD 239745) are also too bright
and saturated in our grism spectra, and the positions of Nos. 77, 230, 12, and 266 are offset
from Kun 53, 73, 170, and 322 by around 10$\arcsec$.
Even if we include these seven stars, only 12\%
of stars can be identified with Kun stars.  The rest of the Kun stars show obvious
H$\alpha$ absorption or no emission, and 10 of them show the spectra of M-type stars in our grism spectra.
Medium resolution spectroscopy by \cite{bal96} show that Kun 193 (No. 340; CepX-4)
exhibits conspicuous hydrogen emission, but 34 other Kun stars do not.
They suggested that the lack of emission is due to the time variability of H$\alpha$ stars.
\citet{con02} failed to detect H$\alpha$ emission in spectroscopic observations of
20 selected Kun stars, only finding emission in Kun 314 S. Thus, they suggest that the original
identification of emission was incorrect. Our result is consistent with their suggestion.

\citet{sic04,sic05}  extensively studied
the low-mass population of the two clusters in Cep OB2, Trumpler 37 and NGC 7160, to investigate
the disk evolution at ages 1--10 Myr.
For Trumpler 37, they have performed optical photometry and multifiber spectroscopy
in a square about 45$\arcmin$ per side, centered at  HD 206267.
Approximately 45\% of the low-mass population indicate NIR excesses,
suggesting heated dust in the circumstellar disk.
Finally, \citet{sic06b} examined the membership using  H$\alpha$ emission, Li $\lambda$6707 absorption lines,
and radial velocities as membership criteria.
They identified accretion properties in 170 members in the central part of IC 1396.
53\% of the members of this list are also detected in our survey.
The  equivalent width of the H$\alpha$ emission-line of our candidates is consistent with that of
\citet{sic05}, except for only a few stars.
We have detected $\sim$ 90\% and  $\la$ 30\%  of  Class-II and  Class-III
objects in their list as H$\alpha$ stars.
This result is naturally explained by the higher detectability of weak emissions
in their high dispersion slit spectroscopy.

Using archival data of {\it Chandra} and {\it Spitzer},
\citet{mer09} have identified 25 X-ray sources as cluster members, which have
MIR colors of CTTS or WTTS in the 10$\arcmin$ $\times$ 8$\arcmin$ region around HD 206267.
Their sources consist of five CTTS and 20 WTTS.
Although four of the CTTS were detected in our observations,
only two WTTS match our H$\alpha$ stars.

\citet{get07} obtained X-ray images of the bright rimmed cloud SFO 38 (IC 1396N) using the
{\it Chandra} ACIS detector.
They identified X-ray sources in the area of a square of 5$\arcmin$ with the {\it Spitzer} IRAC sources
and concentrated their study on 25 sources associated with the globule SFO 38.
Of the 117 X-ray sources, 17 sources are identified with our H$\alpha$ stars and five of these X-ray
sources are associated with H$\alpha$ stars in the SFO 38 cloud.

\subsection{Comparison with {\it IPHAS} Sources }

In the recent paper by \citet{bar11},
they identified 158 PMS candidates in a 7 deg$^2$ area towards IC 1396
by using the data of IPHAS \citep[the Isaac
Newton Telescope/Wide Field Camera Photometric H$\alpha$ Survey; ][]{dre05}.
Out of 143 PMS candidates identified by \citet{bar11} in our field of view,
119 stars are in common with our H$\alpha$ sample.
We examined the common H$\alpha$ stars in IPHAS to confirm our photometric quality.
The IPHAS magnitude is based on the Vega magnitude and hence we converted it to
AB magnitude \citep{gon08}.
\citet{bar11} restricted their sample to sources with
$r'_{IPHAS}$ $<$ 20 mag, which corresponds to
$i'$  $<$ 19 mag if we adopt the colors of known T Tauri stars in their figure 4.
For most of the stars in common, our $i'$-magnitudes are consistent with those in the IPHAS catalog within 0.1 mag.
Although a large scatter ($\sigma$ = 0.3 mag) of the magnitude differences is found, it may be due to
the photometric  variability of young stars.

\citet{bar11} compared their objects with the members confirmed by \citet{sic06b}, and estimate the completeness.
89\% of PMS candidates with the H$\alpha$ EW $>$ 30 {\AA} identified by \citet{sic06b} are
recovered by \citet{bar11}.
We also estimated the completeness of our survey with the same manner.
For the PMS candidates including smaller EW ( $>$ 10 {\AA} ),  the fraction of recovered sources by \citet{bar11}
falls off to 50\%.
On the other hand, the fraction of recovered sources with EW $>$ 10 {\AA} maintains 86\%  (51 out of 59) in our sample.
We confirmed that none of their rejected candidates ( 30 stars ) by \citet{bar11} were included in our list.
Thus, our observations are more sensitive than their survey for the emission-line stars with
small H$\alpha$ equivalent width.

\subsection{Identification with {\it AKARI} Sources }

We identified 27 sources among our H$\alpha$ stars with the sources of  the point source catalog of
the MIR All-Sky Survey obtained with the infrared camera (IRC) on board the {\it AKARI} satellite \citep{ish10},
with position differences of less than 5$\arcsec$.
Table 3 gives the {\it AKARI}  9-$\micron$ ($S9W$) and 18-$\micron$  ($L18W$) magnitudes and their 2MASS photometric data.
Their positions on ($J$--$Ks$) vs. ($S9W$--$L18W$),  ($J$--$Ks$) vs. ($Ks$--$S9W$),  and ($J$--$Ks$) vs. ($Ks$--$L18W$)  diagrams
are shown in Figure 3. The criteria for extracting TTS from these diagrams, proposed by  \citet{tak10},
are also shown as a dashed line (Figure 3a) or areas (Figure 3b,c).
The colors of three stars (Nos. 287, 309, 575) are consistent with cool carbon stars,
and about 20 stars are pre-main sequence stars.
The bright source No. 436 is the candidate for the exciting source of the HH 588 object.
Figure 4 shows the contour map of the number of emission-line stars overlaid on a false-color map
using the IRC on  {\it AKARI}.
Blue is for 9 $\micron$ and red is for 18 $\micron$.
Probable members of 66 B--F stars from  \citet{con02}, supplemented by
8 OB stars from  {\it Hipparcos} results \citep{dez99},
are also shown as filled blue circles.
As for H$\alpha$ stars in  the West and East regions, high or intermediate-mass stars are concentrated
near the center of the large dust cavity, which is presumably swept up by the expansion of the H {\sc ii} region.
We note that their distribution is slightly shifted to the east of HD 206267.

\section{Analysis \& Discussion}

\subsection{Probable Members }

Our list of H$\alpha$ stars in Table 2 may contain foreground or background, magnetically active field stars.
We estimated the number of unrelated main
sequence stars with enhanced chromospheric and coronal activity.
Within the 4.2 deg$^2$ field towards the IC 1396, the Besancon model of the Galactic
stellar populations \citep{rob03} predicts $\sim$4000 and $\sim$ 1700 dM stars down to $V =$ 20 mag
in the foreground and the background (the distance range between 870 and 1500 pc) field, respectively.
Although 44\% of the foreground dM stars are in the range of $V <$ 19 mag, 3\% of the background
dM stars are in the same magnitude range.
Following the same approach as \citet{das05}, we used the
the stellar luminosity function derived by {\it Hipparcos} \citep{jaw97}
and the dMe (with an H$\alpha$ EW $>$ 1 {\AA}) incidence from the nearby star survey of
\cite{haw96}.
We adopted a completeness limit for the present observations of $V =$ 20 mag.
We assumed the scale height of 325 pc for an exponential falloff in the space density, and
0.7 mag kpc$^{-1}$ for the diffuse absorption.
The estimated number of dMe stars in the foreground and the background (up to 1500 pc)  is 193 and 33
in our observed area, respectively.
The total number of  the field dMe stars, 54 per square degree, is consistent
with the average number density of H$\alpha$ stars in the field area, 58 per square degree.

It is also possible that there is contamination by pre-main sequence stars associated with
the foreground cloud \citep{pat95,wei96}.
As the AKARI 9 $\micron$ image, which traces the photodissociation region in the periphery of the H {\sc ii} region (Figure 4),
is likely to be dominated by polycyclic aromatic hydrocarbons (PAHs)
emission features,
H$\alpha$ stars associated with 9-$\micron$ emission are not likely to be foreground objects.
The dark clouds B 163 and B 163SW do not show any sign of bright rims and their radial velocities of
the molecular emission line are 6 km s$^{-1}$ \citep{pat95}.
The radial velocities of the other associated globules are between $-9$ km s$^{-1}$ and $+2$ km s$^{-1}$.
From the radial velocity, \citet{leu82} suggested 150 pc for the distance of B 161, which  also shows no
bright rims and no indication of heating from behind \citep{wei96}.
The broad, curved dark lane Kh 161 \citep{kha60} and inverse S-shaped B 365, both of which show weak and diffuse emission
at the northern and southern part of Figure 1, appear in foreground clouds.

Figure 5 illustrates the NIR color--color diagram of our emission-line stars.
The solid lines yield the locus of the main-sequence and of the giant branch
according to \citet{bes88}, while the dash-dotted straight line indicates the locus
of the unreddened CTTS following \citet{mey97}.
We used the color transformation equations of \citet{car03} to convert their loci into the 2MASS  system.
The reddening vector adopted from \citet{coh81} is also shown.
We selected nearly 40\% of the H$\alpha$ stars whose NIR colors are consistent with the colors of
the reddened CTTS in Figure 5 and calculated the source extinction by
tracing back along the reddening line to the CTTS locus.
In the above procedure, we have not separated between WTTS and CTTS candidates,
and  treated all H$\alpha$ stars as the same way.
Although generally an unreddened WTTS does not show the color of the CTTS but rather of the normal main sequence,
most WTTS have NIR colors of K- to early M-type stars, i.e.,  ($H$--$Ks$, $J$--$H$) $\sim$ (0.2, 0.64),
that is close to the locus of unreddened CTTSs.
Thus, we have not lost many WTTS in the above procedure.
Three carbon stars, discussed in the previous section and shown as open circles in Figure 5,  are excluded.
Figure 6 shows a histogram of the measured extinction of 252 stars excluding three carbon star candidates
(see \S 3.3) and No. 250/251.
The median value of the source extinction is $A$v$=$1.74 mag.
This value is consistent with the average extinction $A$v$=$1.56 mag obtained by \citet{sic05} for Trumpler 37.

The high mass stars in our surveyed area are two O-type stars,
HD 206267 (O6) and HD 206183 (O9.5V),  and six early B stars (B0--B5) \citep{dez99}.
When Rv$=$3.1, the foreground extinction of these OB stars should be  1.3--2.1 mag \citep{gar76}.
\citet{con02} excluded stars with $A$v $<$ 1.0 mag as foreground stars and
excluded stars with  $A$v $>$ 2.3 mag as background objects.
As the background contamination by field dMe stars is not so high,
many of the emission-line stars  with $A$v $>$ 2.3 mag in our survey appear to be associated with
dark clouds or globules.
Therefore, we selected 189 stars with $A$v $>$ 1.0 mag as likely members associated with IC 1396.
Most known T Tauri stars  \citep[e.g., ][]{sic06b}  in Table 2 have $A$v $>$  1.0 mag, but 12 T Tauri stars have low
extinction, and more than half of them are located near HD 206267.

Figure 7 shows a histogram of the measured equivalent width.
The fraction of weak (EW $<$ 10 {\AA}) emission-line stars among the IC 1396 PMS candidates
is low (27\%)  relative to that over the entire sample  (44\%).
It appears that the fraction of CTTS candidates among the PMS candidates in the IC 1396 region is higher than that among
the candidates proposed as foreground (or background) objects.
We could not find any evidence of the difference between the spatial distribution of
CTTS and WTTS.

To identify the HAeBe stars, which have larger infrared excess than CTTS,
we adopted the extended criteria in the NIR color--color diagram proposed by \citet{lel08}.
They used the region between two parallel reddening lines on their figure 4 and above ($J$--$H$) $>$ 0.2 mag to
pick up HAeBe stars, excluding  B[e] and classical Be stars
from the young star sample as contaminants.
According to their criteria, we selected five stars, redder than the reddening line passing through the truncated point of
the CTTS locus and $J$--$H$ $>$ 0.2 mag, including a known HAeBe, MVA-426 \citep{sic06b}.
It is suggested that from their  $J$ magnitudes  Nos. 13, 236, and 606 are HAeBe stars and
No. 479 and 545  are Class-I objects.
In the following discussion, we have added these stars and 12 T Tauri stars with low extinction to the probable members
totaling 205 stars.
The number of new unpublished PMS candidates identified in the current survey is 72
including three Class-I objects or HAeBe stars.

Figure 8 illustrates the contour map of the number density of emission-line stars associated with IC 1396.
Dashed boxes represent the eight subregions,  namely, the East, West, SFO38, SFO37, SFO39/41, Rim B,
Halo, and Field regions.
Their distribution is not very different from Figure 2, though
the peak of the distribution at the East region is slightly shifted westward.
While the aggregate at the north of B 365 (see Figure 1), which is shown in Figure 2b,  disappears in Figure 8
and therefore could be a foreground object,
other aggregates should be associated with IC 1396.
Table 4 summarizes the number of emission-line stars in each region.
The H$\alpha$ stars, whose $A$v values we could not obtain,  appear to be spread over the observed field rather uniformly.
Thus, we suggest a large number of them are field stars.

\subsection{Ages and Masses of H$\alpha$ stars}

\citet{mar90} determined that the time after the first stars reach the main-sequence is 7 Myr in Trumpler 37 and
\citet{sic05} confirmed 4 Myr for the age of Trumpler 37
from optical photometry and theoretical isochrones.
The expansion of the H {\sc ii} region creates a swept-up shell and results  in a compressed molecular ring around its periphery.
From the size of the ring, \citet{pat95} suggested a dynamical age of the system of globules of 2--3 Myr.

Figure 9 shows the extinction-corrected $i'$ vs. ($i'$--$J$) diagram of the 194 probable members
with $i'$-band data, using
the $i'$-band extinction correction from \citet{cad89}.
Here, we adopted the pre-main sequence model  of \citet{sie00}.
Their effective temperature and luminosity are converted into our system
using the table of \citet{ken95} and the equation of \citet{jor06}.
In Figure 9, the 0.1, 1, 3, 5, 10, and 100 Myr isochrones
are overlapped as well as  the evolutionary tracks for masses from 0.1 to 2.0 M$_{\sun}$, at an
assumed distance of 870 pc.
As the reddening vector runs almost parallel to the isochrones,
the extinction value would not severely affect our age estimate.

The uncertainty of the distance modulus (8.94--9.70)  and the choice of PMS models
affects the estimation of ages and masses of  H$\alpha$ stars from Figure 9.
We used the pre-main sequence models of \citet{pas99}, which are converted to our
photometric system by a table of \citet{ken95} and the equation of \citet{jor06}, for comparison.
By assuming the nearest distance, 615 pc \citep{dez99}, the evolutionary tracks shift upwards, and it
makes the age $\sim$0.2 dex older in both models.
The age and mass histograms of the probable members in different choices of PMS models
adopting 870 pc are shown in Figure 10.
They indicate that the numbers of young stars ( $<$ 1 Myr ) predicted from the Siess models
(Fig 10a) are generally smaller than those predicted from the Palla \& Stahler models (Fig 10b).
On the other hand, the number of  low mass stars ( $<$ 0.4 M$_{\sun}$) derived from the Siess models
(Fig 10c) are slightly large compared to those derived from the Palla \& Stahler models (Fig 10d).
We should notice the incompleteness of our PMS candidate sample along with possible effects on the
distribution of masses and ages.
\citet{dar10}  carefully investigated the stellar population of the Orion Nebula Cluster by using these two
PMS models.
The completeness function in the mass-age plane, derived from their statistical simulation for
two evolutionary models, shows that a large incompleteness correction is needed in the low mass ($<$ 0.2 M$_{\sun}$) range.
They  attributed the difference of results  to the different shapes of tracks and isochrones in this mass range.
Although we adopted the Siess models, the uncertainties would be larger for stars with ages  $<$ 1 Myr and masses $<$ 0.2 M$_{\sun}$.
Furthermore, we could not detect emission-line stars near the region of higher obscuration such as the globules,
and within 1$\arcmin$  of  the bright O star HD 206267, due to
saturation of the detectors,  light contamination from this star, and diffraction spikes from this star.

Table 5 shows the number of H$\alpha$ stars in each age and mass bin in Figure 9.
The age and mass histograms of H$\alpha$ stars in each subregion are shown in Figure 11.
We combined the SFO37/38/39/41/Rim B regions in the  BRC (bright-rimmed cloud) region.
Most of the H$\alpha$ stars have ages of $<$ 3 Myr and masses of 0.2--0.6 M$_{\sun}$.
The number of stars with an age less than 1 Myr and with an age of 1--3 Myr are
comparable in the region associated with bright rims, i.e., the BRC region.
We confirmed that the above result is also true for the age assigned from the Palla and Stahler model,
and is not dependent on the choice of distance.
The histogram in the West region is similar to that of the BRC region,  probably because
most of the H$\alpha$ stars  in the West region are associated with Rim A.

From the extensive survey of young stars  by {\it Spitzer}, \citet{koe08} found two distinct
generations of star formation in W5.
They considered two triggered star formation mechanisms, radiative driven implosion \citep[RDI; e.g.,][]{mia09} and collect-and-collapse,
to explain their findings and concluded that both mechanisms are at work in the W5 H {\sc ii} region.
\citet{deh10} extensively studied the nature of infrared bubbles which enclose H {\sc ii} regions and discussed
star formation triggered by the expanding H {\sc ii} region at their edges.
They show that most of these bubbles enclose H {\sc ii} regions ionized by O--B2 stars, many are formed to be
surrounded by cold dust shells (good candidates for C\&C processes),
and many have bright-rimmed dust condensations protruding inside the H {\sc ii} region
(good candidates for RDI process).
In the IC 1396 region, the presence of aggregates associated with the bright rims immediately inside the
IC 1396 H {\sc ii} region or the near side of the ionizing
star HD 206267, such as the West (Rim A), Rim B, and SFO38 regions, suggest that the star formation
in these regions has advanced away from HD 206267 in $<$ 3 Myr.
Such a configuration is consistent with squeezing of the pre-existing condensations compressed
by the pressure of the ionized gas.
The kinematical structure of  SFO 37 \citep{sug97,ike08} and an X-ray study of SFO 38 \citep{get07} also favored
the  RDI model.

\subsection{Star Formation in the Central Region}

In our previous results  for the W5E H {\sc ii} region \citep{nak08},
we have found three aggregates of H$\alpha$ emission-line stars in the W5E H {\sc ii} region.
Two of them are located at the edge of the H {\sc ii} region, and one is near the central exciting O7 star.
The former two aggregates are systematically younger than the latter.

Based on a comparison of the stellar ages in the BRC region with those in the East region of IC 1396 (Figure 11),
it might appear  that the low-mass population in the East region is older.
We only find two stars younger than 1 Myr  in the East region, in contrast to the West region.
It may suggest that the star formation activity in the East region has ceased recently.
As there remains no molecular material associated with the population in the East region,
the exciting star HD 206267 has already dissipated the natal molecular cloud.
However, a Kolmogorov-Smirnov (K-S) test gives a probability of $>$ 15 \%
that the two samples have the same distribution in age, even if we choose either PMS model.
The difference between the ages of H$\alpha$ stars in the BRCs region and the East region is not
statistically significant.

\citet{sic06a} estimated ages for six members near Rim A or in the globule.
They found that the ages of five stars are younger than 1 Myr, which is significantly lower
than the average age of Trumpler 37.
Figure 12 plots the spatial distribution of H$\alpha$ stars with derived ages.
At a glance, younger stars in Figure 12a are preferentially  located at the West region
compared to those at the East region.
Again we used K-S test to compare the distribution in right ascension and declination derived from
different choice of PMS models.
A probability that  two samples of different age (Fig 12a and 12b)  have the same distribution in
two coordinate axis is  $>$ 25 \% and $>$ 54 \%.
Thus, the age difference of young stars in the West and the East region is not statistically clear from the spatial distribution of our sample.

In addition to the West region, Figure 12b shows a number of stars with an intermediate age  (1--3 Myr)
in the East and SFO38 regions, extending to  the Halo region.
A linear sequence of young stars across the center is noticeable.
A filamentary dark cloud extends from Rim A to the western rim of the H {\sc ii} region.
It is noteworthy that H$\alpha$ stars are distributed along this structure and further extend to the east of
HD 206267.  This spatial distribution strongly suggests a
fossil record of a star forming cloud including Rim A and B.

\citet{sic05}  argued a spatial east--west asymmetry in the young low-mass members of Trumpler 37,
compared with more massive ones \citep{con02}.
The same spatial asymmetry with respect to the central ionizing O star, HD 206267,  was seen
in the distribution of the {\it Spitzer} IRAC excess objects \citep{sic06a}.
The asymmetry of H$\alpha$ stars with high disk fraction may be explained by
photo-evaporation of the disk material around the forming stars by strong UV radiation.
\citet{sic05} suggested that the interstellar material, lying between powerful O6 stars and
young stars with disks, shields the disk from UV radiation.
However, there is no evidence of such an asymmetry of interstellar material from  molecular line \citep{pat95}
and millimeter dust continuum observations \citep{ros10}.
Actually, significant destruction of disks occurs for stars located out to distances
of $<$ 0.5 pc, which corresponds to only a few arcmin from HD 206267, as found in NGC 2244 \citep{bal07}.
\citet{sic05}  additionally suggested probable age differences for the explanation for the asymmetry in the
CTTS distribution.
Instead of disk photo-evaporation,
we prefer that this spatial asymmetry represents the star formation sequence.
If most of the young low-mass population in the West region was formed as a result of a triggered event,
those in the East region could be formed along with massive stars.

\subsection{Star Formation in the BRC Region}

There are 116 probable members of emission-line star in the BRC region including the West region, and
the total mass  is about  60--70 M$_\sun$.
If we add 35 emission-line stars in the East region,  the total mass reaches 70-90  M$_\sun$.
Since  our survey is biased toward the region of low extinction,
the above estimates of the number and mass of the low-mass population in the BRC region including the West and the East region
should be considered the lower limits.
For example, \citet{cho10} found $\sim$45 YSOs in and around SFO 38, where we could not detect any
H$\alpha$ stars in the globule.
Of these, 26 sources are Class-0/I, Class-I, and Class-I/II, but there are no such objects
situated outside the ionized rim.
It follows that the birth of low-mass stars associated with bright rims appears to be the primary mode of
star formation in IC 1396 at present.

The higher mass O--F stars of Trumpler 37 \citep{dez99,con02}
total $\sim$ 200 M$_\sun$ in our observed fields (Figure 4).
Assuming  the initial mass function of \citet{kro01}  between 0.01 M$_\sun$
and 50 M$_\sun$, we estimate the total mass of stars in Trumpler 37 to be $\sim$ 500 M$_\sun$.
Young low-mass stars, which probably formed by a triggered mechanism in the BRC region,
contribute a fraction of the mass of stars in IC 1396.

\subsection{The Birth of HD 206267}

\citet{ike08} has determined the alignment of YSOs and their age gradient at the tip of SFO 37.
They argued that this alignment and the elongation of the head of the globule are
attributed to UV radiation from the O9.5V star, HD206183, at their formation stage.
The dominant exciting source, however, is currently HD 206267.
Consequently, HD 206267 formed  at the late stage of star formation
in the central part of the H {\sc ii} region and disrupted the natal molecular cloud.
\citet{bar11} reported the age gradient of the PMS candidates along the distance from this hot star.
Their results also favors the triggered formation of stars in IC 1396.
HD 206267 is known as the Trapezium system of OB stars with a maximum separation of 15000 AU,
and the main component A is a triple \citep{sti95}.
\citet{bmm97} confirmed the observed masses and evolutionary model masses
and suggested that the two bright components of the triple are O6.5 V((f))  (A$_1$) with 38--61 M$_\sun$
and O9.5: V (A$_2$) with  17--28 M$_\sun$.
Therefore, the age of HD 206267 is estimated to be $<$ 3 Myr from the main sequence lifetime \citep{sdk97}.

Numerical simulation considering protostellar outflow-driven turbulence has been discussed
by \citet{lin06} and \citet{nal07}.
Following their study, we suggested that the massive exciting star of the
W5 E H {\sc ii} region was possibly formed after the continuous production of stars  \citep{nak08}.
The birth of the most massive star should be the last stage of star formation.
The  contiguous formation of stars for 10 Myr in Trumpler 37 could be supported by Figure 12.
Many of  the low-mass stars near  Rim A and SFO 38 might be formed in $\la$ 3 Myr.
As there is no conspicuous molecular material except the elephant trunk globule, Rim A,
in the evacuated dust cavity   (Figure 4),
HD 206267 was likely born in the central part after the continuous low mass star formation.
It is reasonable to suppose that the formation of massive stars and the associated low-mass
population in Trumpler 37, continued for a few Myr.
Although it is difficult to separate the low-mass stars formed as the same generation with HD 206267
and formed by the trigger mechanism of HD 206267,
we believe that many of H $\alpha$ stars at the rim were triggered to form by a radiation driven implosion
mechanism after the formation of HD 206267.

\section{Summary}

We have made an extensive survey of emission-line stars in the IC 1396 H {\sc ii} region to  investigate
the low-mass PMS population  near the OB stars.
A total of 639 H$\alpha$ stars were detected over a 4-deg$^2$ area and their $i'$-photometry was performed.
Their spatial distribution shows several aggregates near the bright-rimmed clouds at
the center and the edge of the H {\sc ii} region (Rim A/B and SFO 37, 38, 39, 41) and one near the main exciting star
of the H {\sc ii} region.
Based on the source extinction estimated from the NIR color--color diagram, we have selected PMS candidates
associated with IC 1396. The age and mass were derived from the extinction corrected color-magnitude diagram
and theoretical evolutionary tracks.
Most of the H$\alpha$ stars have ages of $<$ 3 Myr and masses of 0.2--0.6 M$_\sun$.

The spatial distribution of the PMS candidates indicates that the stellar population in the East region
is spatially distinct from that in the West region, associated with Rim A globule.
The age difference between two populations was also suggested by \citet{sic06b, bar11}.
The spatio-temporal gradients of the stellar age were also demonstrated near the bright-rimmed
clouds by \citet{get07, ike08, cho10}.
Our K-S test does not support the significant difference between ages of two populations.
Also, the spatial distribution of  $<$ 1 Myr stars is not significantly different from the distribution of
1--3 Myr stars.
Although the star formation activity in the East region could be low in the last 1 Myr,
we need further confirmation.

The linear sequence of stars including the West (Rim A) region and Rim B region, which is conspicuous in
Fig 12b  of 1--3 Myr age across the center of the H {\sc ii} region, suggests a fossil record of the star
forming cloud.
The formation of massive stars and associated low-mass population of Trumpler 37
continuing for a few Myr, and
the most massive star in Trumpler 37, HD 206267, was likely born $\la$ 3 Myr ago.
Then, the IC 1396 H {\sc ii} region was formed by strong UV radiation.
In the last stage, the H {\sc ii} region presumably triggered the formation of low-mass stars in the dense
inhomogeneity.
Our results may suggest that massive stars were born after the continuous formation
of  low-mass stars for 10 Myr.
The birth of the exciting star as the most massive one could be the late stage of
slow but contiguous star formation in the natal molecular cloud.
It presumably triggered the formation of  many low-mass stars at the
dense inhomogeneity in and around  the H {\sc ii} region  by a radiation-driven implosion.
Spectroscopic followup of our PMS candidates to establish their membership correctly
and identify their nature  is needed to clarify the star formation history of
this region.

\acknowledgments

The authors were supported by NAOJ for the use of the UH 2.2-m telescope for the observations.
This research made use of the NASA/IPAC Infrared Science Archive, operated by the
Jet Propulsion Laboratory,
California Institute of Technology, under contact with the National Aeronautics and Space Administration.
This work was supported in part by a Grant-in-Aid for Scientific Research B (20403003) from the
Ministry of Education, Culture, Sports, Science and Technology.

redpajama_set_name: RedPajamaArXiv


text:
The Investment Logic of N5Capital behind the lead in the D1 round financing for FlashEx
由 N5Capital 发表于 September 10, 2018
At the end of August, the same city one-hour express delivery brand FlashEx announced the completion of the $60 million D1 round of financing. N5Capital, Haisong Capital and V Star Capital are the joint leaders of this round of financing.
"As an early-stage investment institution,FlashEx is not the sweet spot for our usual investment. First, because the investment amount is relatively large; second, the investment phase is relatively late." Will Jiang, founding partner of N5Capital, said.
However, N5Capital still chooses to take the role of the lead investor and participated in the D1 round financing for FlashEx. For N5Capital, what kind of growth potential does it see in FlashEx? In the field of consumption, what is the layout and logic of N5Capital?
FlashEx still has more than ten times growth potential
N5Capital was established in 2013, focusing on early stage (primarily A round) investment in the fields of Consumer & Technology Convergence, fintech and digital economy. At present, N5Capital manages two RMB funds and two US dollar funds, with a management scale of 4 billion yuan and more than 80 projects.
Will Jiang and FlashEx CEO Peng Xue are EMBA students from PBC School of Finance, Tsinghua University, but they really know each other because of the introduction of Muqing Li, an early investor of FlashEx. Muqing Li invested in the A round of FlashEx at the time of CDH Investments. After leaving CDH Investments, Muqing Li and Wenjiang Chen set up YI capital, and made subsequent rounds of investment in FlashEx.
"After our contact with FlashEx, we found that the team really has its own unique features, including the overall pricing strategy, the support of technology for distribution, and the management of crowdsourcing distributors," said Will Jiang.
According to the research of N5Capital, the current same city express delivery market has tens of millions orders per day, and the compound growth rate of the market is around 20%. In the future, it is possible that there will be billions of orders every day. FlashEx cuts into the one-hour express delivery market, which accounts for 10%-20% of the same city express delivery market.
Due to the high requirements on timeliness, the customer base is less sensitive to price. Relatively speaking, customers with high unit price or urgent and important items, users will use the high-end delivery service provider such as FlashEx. For example, files and so on, there are also individual users who have delivered a million-dollar antiques by FlashEx.
"From this point of view, FlashEx is no longer a simple logistics infrastructure, but a consumer brand that goes deep into the C-end. Now the one-hour courier is almost synonymous with FlashEx, and that's one of the things that we value very much. Apart from SF, few other distribution companies have built this kind of brand influence in users' minds. " Will Jiang said.
N5Capital is mainly focused on early stage investments. This time, there are also strategic consideration behind breaking the usual routine and participated in the D1 round financing of FlashEx. Will Jiang said that N5Capital had invested in Hot & Hot, Soup Town and other companies in consumer sector. Hot & Hot and FlashEx have already started collaboration in delivery service under the introduction of N5Capital. Will Jiang believes that the one-hour distribution network may become an indispensable infrastructure for consumer products in the future, and FlashEx has the value and opportunity to cooperate with consumer companies invested by N5Capital.
In terms of the company's financial performance, FlashEx said that after the company's business was launched in 2014, it achieved profitability in 2016, and then maintained a growth rate of 300% per year. After the current round of financing, the company's cash reserves have reached 150 million US dollars.
"This kind of cash reserve means that FlashEx is not afraid of any new entrants. On the other hand, everyone is talking about capital winter, so it is a wise choice to have more cash reserves." Will Jiang told 21Jingji.com. Currently, FlashEx has basically become synonymous with the "one-hour express delivery". In the next two years after this round of financing, the company will enter a high-speed growth period and gain more than 10 times growth, becoming a company with at least the same level as the "Shentong Express, Yuantong Express, Zhongtong Express, Huitong Express, Yunda Express".
Investment in Consumption sector should pay attention to technological value
FlashEx is just one example of N5Capital's investment in the consumer sector. In addition, N5Capital has invested in companies such as TalkingData, 360 Finance, Hot & Hot, Shilily, Rent to Play, Zhulogic, and Soup Town, etc. Among them, N5Capital's 10 million RMB angel investment TalkingData is expected to be listed in the near future, bringing about a return of 100 times for N5Capital.
"Most consumer companies are doing straight-line business and copying from one point to another. N5Capital wants to invest in consumer companies that use technological progress to bring curve growth." Will Jiang told 21Jingji.com.
He said that when N5Capital invests in the consumption field, the key points are the right place, the right time and the right people.
"The right time" refers to the market size. It is possible that any consumer segment in China can achieve a market size of 100 billion yuan. However, N5capital wants to invest in sectors that are on the rise, with compound growth rates of two to three times the GDP growth.
"In addition, we hope to invest in a relatively fragmented market. No one in the market can achieve a market share of more than 1%. The supply and demand sides are scattered. There is a need for integration in this industry, and technology can generate more value," he said.
"The right place" refers to the value brought by technology, that is, the increase in gross profit margin. Will Jiang said that gross profit comes from the pricing power of the supply side and the demand side, and only technology can generate pricing power. Therefore, when N5Capital invests in the consumption sector, it will use gross profit margin as a prerequisite for measuring whether technology can be effectively used. Of course, if there is no understanding of the upstream and downstream relations of the industry, there is no use of technology, thus the combination of technology and industry is very important.
"The right people" means that the team needs complementary advantages and high human efficiency. The profits of many traditional consumer industry come from squeezing the wage costs of low-end workers.However, the cost of technology focused consumer enterprises will change to some extent.
For example, FlashEx takes advantage of the crowdsourcing scenario. Most of the company itself is a technician, doing algorithm upgrades and pricing strategies, and the profitability is brought up by the improvement of human efficiency. Under these standards, the consumer companies invested by N5Capital have higher gross profit and stronger profitability, and the companies are growing at a rapid rate.
In the financial sector, Will Jiang said that cross-border finance is the trend, but the capital exchanges and related financial technologies in cross-border transactions still remain on the network established more than a decade ago or decades ago.
Although the emergence of Alipay and WeChat have solved the front-end upgrade of cross-border transactions, the cross-border clearing at the back-end has not been upgraded. There are both technical and licensing issues that need to be resolved. "This is also an opportunity for Chinese entrepreneurs. A large part of our investment in the financial sector is in cross-border financial services." Will Jiang said.
In addition, financial derivatives are also N5Capital's investment sector. Will Jiang has had experience in derivatives hedging in Canada. He said that many people in China regard finance as a leverage tool, but the greater role of finance is to hedge the uncertainty and volatility in the real economy. The value of finance as a hedging instrument has been ignored by most entrepreneurs and financial practitioners in the past, but the change has arrived.
"Finance is inseparable from consumption. What we are looking for is the combination of consumption and finance. Recently we have invested in financial derivatives, and these companies have grown beyond our expectations. This is an important opportunity for new fintech companies." He said.
In the digital economy, Mr. Jiang says that while China's mobile Internet dividend is fading, there are still opportunities for the international market. China has the advantage of leading the global market in social network, video and other aspects.(Text: 21Jingji.com. Reporter Shen Junhan/Editor Lin Kun)
No.16 Jia, BeiXinCang Hutong, DongCheng District, Beijing
info@n5capital.com
WeChat QR Code
Copyright © 2018 N5Capital. All rights reserved.

redpajama_set_name: RedPajamaCommonCrawl


text:
Livres anglais >
Why Lhasa de Sela Matters
Par Fred Goodman
Éditeur University of Texas Press
Collection : Music Matters
Papier ISBN: 9781477319628 Pas en stock. 20.95$
An artist in every sense of the word, Lhasa de Sela wowed audiences around the globe with her multilingual songs and spellbinding performances, mixing together everything from Gypsy music to Mexican rancheras, Americana and jazz, chanson française, and South American folk melodies. In Canada, her album La Llorona won the Juno Award and went gold, and its follow-up, The Living Road, won a BBC World Music Award. Tragically, de Sela succumbed to breast cancer in 2010 at the age of thirty-seven after recording her final album, Lhasa.
Tracing de Sela's unconventional life and introducing her to a new generation, Why Lhasa de Sela Matters is the first biography of this sophisticated creative icon. Raised in a hippie family traveling between the United States and Mexico in a converted school bus, de Sela developed an unquenchable curiosity, with equal affinities for the romantic, mystic, and cerebral. Becoming a sensation in Montreal and Europe, the trilingual singer rejected a conventional path to fame, joining her sisters' circus troupe in France. Revealing the details of these and other experiences that inspired de Sela to write such vibrant, otherworldly music, Why Lhasa de Sela Matters sings with the spirit of this gifted firebrand.
Envoûtante Lhasa
Fred Goodman
Venus in the Blind Spot
Pas moi
Harry Potter Box Set: The Complete Co...


StackInsights: What's the top collaboration tool?
In the old days, say the 1990s, employees could get information from internal computer networks or the lunchroom cafeteria. Now with one team member in Boston, one in LA and one in Barcelona, with everyone using their own devices, collaboration tools are needed to keep them working in the same direction.
Collaboration tools do more than help teams working remotely or in different time zones. They support employees who work flexible shifts so they can balance work with a life but need one central place to get the authoritative instructions. They help teams where everyone has his/her own laptop. Or help provide a secure way to build camaraderie and consensus through shared gifs from The Office.
"Because we have access to very good tools in our private lives we expect the same level of functionality and performance in business," said Jeffrey Mann, vice president and analyst at Gartner. He notes that keeping the right collaboration platforms in place help keep a workforce engaged. By 2020, 45 percent of all CIOs surveyed by Gartner said they expect to be supporting Bring Your Own Device programs and only half of them are expected to still be running a corporate device program at all by then.
So, for enterprises managing collaboration tools as part of their marketing technology stacks on CabinetM, what is the most popular collaboration tool?
The most popular is Slack, the tool that started as a platform for development teams sharing snippets of code is now the top choice for enterprises currently building stacks on CabinetM.
Remember, just because a platform is popular doesn't mean it fits in with your particular strategy. Just in the roundup of mobile collaboration tools we see very different capabilities to speak to many different kinds of teams.
If you need help managing your marketing technology stack, Erica Ross in our office is here to help. She's at eross@cabinetm.com.


Religious Fervour in Derby • Cloned Rabbits Begin to Breed • Growing Human Organs for Fun and Profit • Happy Philosophy Day!
Güven Güzeldere asks where we are now with the mind-body problem.
An introduction to our special section by this issue's editor, Charles Echelbarger.
Mark Goldblatt analyses the moral and legal arguments on both sides of America's most divisive issue.
Members of different cultures with different values and beliefs come into frequent conflict, sometimes violent. Exploiter or entrepreneur? Murderer or martyr? "Great Satan" or "Great – Santa!" Gerald Lang asks if we can still pass judgment.
Surveillance cameras watch our every move. They reduce crime and maybe save lives. So why the fuss about privacy? Scott O'Reilly discusses the technologies of control.
Lisa Kemmerer cheers on Tom Regan as he defends the idea of animals having rights.
Chris Bloor found Body Worlds, an unusual show of dead bodies in London, to be essential viewing.
Anna Winestein loathed the Eat Art exhibition at Harvard.


A construction company's organizational structure refers to both the arrangement of job roles and the reporting and operational relationships between and within these roles. A variety of roles and responsibilities – including marketing, purchasing, human resources, finance, pre-construction tasks and construction operations – most often make such a corporate structure organized according to departments, functions or areas of responsibilities most appropriate to organizational design.
Functional departmentalization is an example of a traditional, hierarchical organizational structure. Defining characteristics include horizontal separation of the various departments and functions, well-defined lines of control and top-down communications. For example, authorities and communications flow from the business owner to the management team to project managers or superintendents and finally to rank-and-file construction employees.
A main reason most construction companies group roles that require similar knowledge and skills into a functional organizational structure is that it increases operational efficiency and promotes the development of departmental expertise.
The size of a construction company determines the degree of horizontal separation. Although the business owner assumes a general management role regardless of the size of the business, the business owner's roles and responsibilities are often greater in a small construction company. In addition, while larger construction companies most often include a higher degree of horizontal separation, smaller companies may combine similar roles.
For example, small companies may combine marketing and development, and community affairs into a single business development department, while a larger company might separate these into two distinct departments.
A main disadvantage of a departmentalized organizational structure is that it can lead to situations in which department goals, such as risk management and construction operations, become more important than overall strategic company objectives. In addition, coordination of work efforts across departmental boundaries may become more difficult or confusing the larger a construction company becomes.
Directional communication patterns characteristic of a departmentalized organizational structure may contribute to the development of these situations. For example, horizontal communications most often only take place between staff members of equal or comparable rank, while vertical patterns typically relate to a business's internal chain-of-command. In the absence of a good horizontal communication system, this could lead to lower-ranking project managers or superintendents continually finding themselves answering to multiple senior department heads.
Specific job roles follow the same hierarchical structure, decision-making and communications flow. For example, authorities in a hierarchical structure in the construction operations department might flow from the operations department head to project executives to project managers to project superintendents. The degree of authority, however, depends on company policies and often on the size of the business.
In some construction companies, the project superintendent might focus solely on organizing, planning and scheduling a construction project, leaving all responsibilities associated with site supervision to the project or site manager. In others, however, the project supervisor might take a more direct field supervision role, requiring the project or site manager to follow and administer higher-level decisions.
Lohrey, Jackie. "Organizational Structure of a Construction Company." Small Business - Chron.com, http://smallbusiness.chron.com/organizational-structure-construction-company-77196.html. 25 January 2019.


The background for this blog was obtained from Leelou Blogs. I went with this one as it seems the easiest to use and install. Leelou provide the whole template including headers and buttons so you won't have to add extra code for these features.
There are other places to get backgrounds, and they may have different ways of adding their background templates. I'll stick with this one for this post, but might address the others at a later date. Other sites may also require you to add buttons, headers and other features separately, if indeed they have co-ordinating ones.
The first thing you have to do is make sure you have the correct blogger template to allow you to add a new background. Click on Design and then Template Designer and make sure you have Simple or Minima selected.
Next, you need to go to Leelou and decide which background you want. Then you need to decide if you want a two or three column blog. Select the appropriate blog background by clicking on it.
You then need to click on the 'Grab This Layout' button.
1.Click Save when the pop-up box appears. Save it to somewhere where you can find it again.
2. Go back to your blog and click on Design. Then select 'Edit HTML' and then click the Browse button and locate the file you just saved.
Now click on View Blog and your background and header and any other banners and icons should be there.


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text:
The Reformation and Israel
Some Unfinished Business
Dr. Jürgen Bühler, ICEJ President
Photo: Jews continue to return to a restored Israel (JAFI).
This October 31st marks five hundred years exactly since the start of the Reformation, which dates back to that autumn morning in 1517 when Martin Luther is said to have nailed his 'Ninety-Five Theses' on the doors of the All Saints Church in Wittenberg, Germany. The Evangelical movement today could hardly be imagined without the changes wrought by such reformers as Luther, John Calvin, John Wesley and many other great reformers, who rediscovered old truths of Scripture and thereby helped revive authentic Christianity.
Ever since, the Church has continued to rediscover biblical truths and experience reformation. For example, we have returned to our founding call to world missions contained in the Great Commission. There was a time when most churches did not have a vision for the lost, whether locally or in distant lands around the world. But because of the Moravian brethren and later missionaries like Hudson Taylor and William Carey, nearly every Evangelical church today has a missions budget and other programs that seek to reach the unsaved, both near and far.
Yet there remains one major piece of unfinished business for the Reformation, and that is the Church stills lacks a universal recognition and acceptance of the enduring role of the Jewish people in God's redemptive plans for the world. Luther actually opened the way for this sorely needed change by restoring the Bible to ordinary believers in their native languages, but he also perpetuated traditional Christian anti-Semitism late in his life, hindering the chances for this great re-awakening concerning Israel to take root.
The Israel Reformation
Of all the changes triggered by Martin Luther, his greatest and most lasting impact on the Church was his translation of the Bible from Latin into the common German tongue. This enabled ordinary Christians to once again read and interpret the Word of God for themselves. Previously, it was considered a sacrilege for uneducated lay people even to read the Holy Book. Only the priests and learned could read it, and they often twisted its truths to suit their purposes. But the widespread availability of the Bible would soon transform societies worldwide, as more biblical truths were rediscovered and whole new evangelical church movements were birthed.
As ordinary Christians studied the Bible, they found that one of the great truths of Scripture which had been hidden from them was God's irrevocable covenant with Israel. With few exceptions, most churches down through history had little understanding or appreciation for the divine calling over Israel and the Jewish people. In fact, they taught that God had abandoned the Jews and even cursed them to endless wanderings. They insisted that the Church had replaced Israel as God's redemptive agent in the world, and thus there was no national destiny left for the Jewish people back in their ancient homeland. For centuries, this was the prevailing view in most of the established churches of Europe. Any contrary outlook was brutally silenced. In 1589, one of the first clergyman to write openly about the promised restoration of Israel was the controversial Francis Kett, who was later burned at the stake for a number of heretical beliefs.
Yet today, we are in the midst of a mighty wave of reformation in the Church, and it has to do with Israel. The early Church understood God's enduring purposes for Israel and of our spiritual connection to the Jewish people, and this understanding is being restored to mainstream Christianity today. I believe in coming decades there will hardly be a church which does not have some connection to Israel, and funding a budget to 'bless Israel' will be just as natural as having a mission's budget.
This major shift is taking place because Christians are now aware that God has dramatically changed His own approach towards Israel. The restored Jewish nation testifies to this paradigm shift, exactly as the prophet Zechariah foretold: "'Just as I determined to punish you when your fathers provoked Me to wrath', says the Lord of hosts, 'and I would not relent. So again in these days I am determined to do good to Jerusalem and to the house of Judah...'" (Zechariah 8:14–15)
In other words, God shifts into different gears or phases in His dealings with His chosen people. Over the past 100 years, God has moved from reverse gear to fast forward. Instead of scattering Israel, He is restoring them just as the prophets foretold. No one can overlook any longer this incredible alignment of biblical prophecy and today's events in the Middle East.
This means the teaching of Replacement theology (often masked these days as Fulfilment theology) is being proven wrong by realities on the ground. The reborn state of Israel is a prophetic fait accompli that fully demonstrates the Lord is a covenant-keeping God. And the Church has to come to terms with this new reality. For 1900 years, no one asked: "How do we deal with the restoration of the Jews back to their ancient homeland?" But today we must face this question. This has no parallel in Church history, as no prior generation of Gentile believers had to deal with it. This means the coming years of continued Jewish restoration, both physically and spiritually, will surely be some of the most exciting times in Church history!
Back to our Roots
The good news is that we do not have to invent a new theology. Most of the New Testament was written at a time when there was still a Jewish political entity in the Land of Israel. Therefore, if we look at how the Apostles taught Gentile churches about their relationship to the Jewish people, we will find that the Scriptures are quite clear on how the Church should relate to Israel today.
1. Remember your pagan past
The Apostle Paul first reminded Gentile believers in Ephesus and Rome about their previously hopeless pagan origins. Today, after 2000 years of Christianity expanding to even the remotest parts of the earth, it sounds strange to view ourselves as pagans. But Paul had to remind the church in Rome that as non-Jews, they were like the branch of a wild olive tree. Such wild olive trees produce inedible fruit and thus are little more than a useless shrub.
To the church in Ephesus, Paul appealed: "Therefore remember that you, once Gentiles in the flesh… that at that time you were without Christ, being aliens from the commonwealth of Israel and strangers from the covenants of promise, having no hope and without God in the world." (Ephesians 2:11–12)
Paul also reminds both churches that only after they put their faith in a Jewish Messiah, could they be reconciled to God and become part of His people. Only the book of the Jews, the Bible, gave us hope of knowing a loving God.
This means every Gentile church needs to be humble and mindful regarding their own past.
2. Acknowledge the Hebraic roots of your faith
Paul declares to the church in Rome: "Do not boast against the branches. But if you do boast, remember that you do not support the root, but the root supports you." (Romans 11:18)
That means Gentile Christians should not reject or ridicule the Jewish origins of their faith, but nourish them as one would nourish the roots of a tree. Adam Clark states it so beautifully that through the Jewish people "all the blessing and excellencies which you enjoy have been communicated to you". Or, as Jesus himself declares, "Salvation is of the Jews!" (John 4:22)
This means every New Testament church needs to recognise the role of Israel as a source of "blessing for all the families of the earth" and to respect the Jewish roots of our faith.
3. Appreciate the irrevocable calling over Israel
The New Testament epistles strongly underline the eternal calling over Israel. Even though the Jewish people might not recognise Jesus as their Messiah and might even be 'enemies of the Gospel', Paul still calls them "beloved for the sake of the fathers" (Romans 11:28).
That means if God still loves Israel as is, the Church should love her the same. Paul squarely contradicts every Replacement theologian today: "Will their [the Jews] unbelief make the faithfulness of God without effect? Certainly not! Indeed, let God be true but every man a liar." (Romans 3:3-4)
So even if they are unfaithful, God still is faithful to His covenants, as He cannot deny Himself. Anything else would be a lie.
This means every New Testament church needs to uphold and proclaim the enduring call over Israel.
4. Recognise your spiritual debt to Israel
Paul made clear to Gentile believers that the Jewish people already provided everything necessary for our relationship with God. The Bible is a Jewish book, we serve a Jewish Messiah and it was Jewish apostles who spread the Gospel to the Gentile world. Paul thus declares that Gentile believers are debtors to Israel.
"For it pleased those from Macedonia and Achaia to make a certain contribution for the poor among the saints who are in Jerusalem. It pleased them indeed, and they are their debtors. For if the Gentiles have been partakers of their spiritual things, their duty is also to minister to them in material things." (Romans 15:26–27)
This means every New Testament church needs to be very intentional in how we return the blessings received through the Jewish people.
5. Expect the restoration of Israel
In the New Testament, the Apostles not only affirm the enduring calling over Israel, but they strongly encourage the hope of Israel's restoration. This is demonstrated in the last question they posed to Jesus before his ascension: "Lord, will you at this time restore the kingdom to Israel?" (Acts 1:6)
Paul also conveys this hope to the church in Rome: "For if their being cast away is the reconciling of the world, what will their acceptance be but life from the dead?" (Romans 11:15) In other words, he maintains that a great calling and blessing still lays ahead for Israel.
This means every church should embrace a theology of hope regarding Israel and support her full restoration.
Connect with Israel!
Just as the vision for world missions was renewed within the Church, there needs to be a reformation which reconnects the Church with its Jewish roots. In times to come, a healthy church can no longer afford to ignore Israel. This needs to be taught from every pulpit and become an integral part of the activity, prayers and giving of every church. We see this happening around the world. Join with pastors and believers from around the world in this exciting and historic journey. It is time to complete the unfinished Reformation!
ICEJ's Aid Work in the Year Ahead
ICEJ supports Israeli social entrepreneurs
ICEJ assists with first Aliyah flight of New Year
ICEJ helps sponsor latest Aliyah flight of Bnei Menashe
ICEJ provides Christmas & Hanukkah aid through Arab churches
Time to Rescue the Ethiopian Remnant
ICEJ Supports 'Quiet Aliyah' From Countries in Distress
ICEJ welcomes Ethiopian Jews arriving in urgent airlift
Envision 2021


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text:
The Free Library > Business and Industry > Business > The Journal (Newcastle, England) > August 17, 2012
The Free Library > Business and Industry > Business, international > The Journal (Newcastle, England) > August 17, 2012
The Free Library > Communications > News, opinion and commentary > The Journal (Newcastle, England) > August 17, 2012
The Free Library > Date > 2012 > August > 17 > The Journal (Newcastle, England)
Che Guevara's daughter to give a talk.
Page/Link:
<a href="https://www.thefreelibrary.com/Che+Guevara%27s+daughter+to+give+a+talk.-a0299912812
MLA style: "Che Guevara's daughter to give a talk.." The Free Library. 2012 MGN Ltd. 21 Jan. 2020 https://www.thefreelibrary.com/Che+Guevara%27s+daughter+to+give+a+talk.-a0299912812
Chicago style: The Free Library. S.v. Che Guevara's daughter to give a talk.." Retrieved Jan 21 2020 from https://www.thefreelibrary.com/Che+Guevara%27s+daughter+to+give+a+talk.-a0299912812
APA style: Che Guevara's daughter to give a talk.. (n.d.) >The Free Library. (2014). Retrieved Jan 21 2020 from https://www.thefreelibrary.com/Che+Guevara%27s+daughter+to+give+a+talk.-a0299912812
THE daughter of a left-wing hero will speak about her father's extraordinary life during a visit to Tyneside later this year. Dr Aleida Guevara March, whose father was Marxist revolutionary Ernesto "Che" Guevara, will reminisce about her father when she appears in Newcastle next month.
Dr Guevara will speak at a public meeting on Cuba's achievements in the face of the United States' economic blockade.
This year marks the 50th anniversary of the blockade and the 45th anniversary of Che's assassination by CIA-backed troops in Bolivia.
Dr Guevara has worked as a physician in Angola, Ecuador, and Nicaragua.
She is visiting the UK in September in a speaking tour organised by the Cuba Solidarity Campaign.
Che Guevara was a revolutionary leader who became a left-wing hero and was instrumental in the Cuban revolution which brought Fidel Castro to power. He later fought in the Congo and in Bolivia, where he was killed.
A photograph of him by Alberto Korda became one of the most iconic images of the 20th Century and he has been cited as a hero by figures including Ex-President of South Africa Nelson Mandela and writer Graham Greene.
The Remembering Che tour will come to the Newcastle Civic Centre Banqueting Suite on September 12 between 6pm and 7.30pm. The doors open at 5pm.
Go to www.cuba-solidarity.org.uk for details.
COPYRIGHT 2012 MGN Ltd.
No portion of this article can be reproduced without the express written permission from the copyright holder.
Copyright 2012 Gale, Cengage Learning. All rights reserved.
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The Journal (Newcastle, England)
I can sit thinking 'woe is me' or get out and live my life; Maggie sings again for Charlie Bear after being diagnosed with cancer.
Heartbroken after right-to-die defeat; Judges say no to 'dignified suicide' plea.


Christ admonisheth the people to follow the good doctrine, not the evil examples of the scribes and Pharisees.
Matthew 23:1 Then Jesus spake to the multitudes, and to his disciples, Matthew 23:2 saying, 'On the seat of Moses sat down the scribes and the Pharisees; Matthew 23:3 all, then, as much as they may say to you to observe, observe and do, but according to their works do not, for they say, and do not; Matthew 23:4 for they bind together burdens heavy and grievous to be borne, and lay upon the shoulders of men, but with their finger they will not move them.
His disciples must beware of their ambition.
Matthew 23:5 'And all their works they do to be seen by men, and they make broad their phylacteries, and enlarge the fringes of their garments, Matthew 23:6 they love also the chief couches in the supper, and the chief seats in the synagogues, Matthew 23:7 and the salutations in the market-places, and to be called by men, Rabbi, Rabbi. Matthew 23:8 'And ye—ye may not be called Rabbi, for one is your director—the Christ, and all ye are brethren; Matthew 23:9 and ye may not call [any] your father on the earth, for one is your Father, who is in the heavens, Matthew 23:10 nor may ye be called directors, for one is your director—the Christ. Matthew 23:11 And the greater of you shall be your ministrant, Matthew 23:12 and whoever shall exalt himself shall be humbled, and whoever shall humble himself shall be exalted.
Matthew 23:13 'Woe to you, Scribes and Pharisees, hypocrites! because ye shut up the reign of the heavens before men, for ye do not go in, nor those going in do ye suffer to enter. Matthew 23:14 'Woe to you, Scribes and Pharisees, hypocrites! because ye eat up the houses of the widows, and for a pretence make long prayers, because of this ye shall receive more abundant judgment. Matthew 23:15 'Woe to you, Scribes and Pharisees, hypocrites! because ye go round the sea and the dry land to make one proselyte, and whenever it may happen—ye make him a son of gehenna twofold more than yourselves. Matthew 23:16 'Woe to you, blind guides, who are saying, Whoever may swear by the sanctuary, it is nothing, but whoever may swear by the gold of the sanctuary—is debtor! Matthew 23:17 Fools and blind! for which [is] greater, the gold, or the sanctuary that is sanctifying the gold? Matthew 23:18 'And, whoever may swear by the altar, it is nothing; but whoever may swear by the gift that is upon it—is debtor! Matthew 23:19 Fools and blind! for which [is] greater, the gift, or the altar that is sanctifying the gift? Matthew 23:20 'He therefore who did swear by the altar, doth swear by it, and by all things on it; Matthew 23:21 and he who did swear by the sanctuary, doth swear by it, and by Him who is dwelling in it; Matthew 23:22 and he who did swear by the heaven, doth swear by the throne of God, and by Him who is sitting upon it. Matthew 23:23 'Woe to you, Scribes and Pharisees, hypocrites! because ye give tithe of the mint, and the dill, and the cumin, and did neglect the weightier things of the Law—the judgment, and the kindness, and the faith; these it behoved [you] to do, and those not to neglect. Matthew 23:24 'Blind guides! who are straining out the gnat, and the camel are swallowing. Matthew 23:25 'Woe to you, Scribes and Pharisees, hypocrites! because ye make clean the outside of the cup and the plate, and within they are full of rapine and incontinence. Matthew 23:26 'Blind Pharisee! cleanse first the inside of the cup and the plate, that the outside of them also may become clean. Matthew 23:27 'Woe to you, Scribes and Pharisees, hypocrites! because ye are like to whitewashed sepulchres, which outwardly indeed do appear beautiful, and within are full of bones of dead men, and of all uncleanness; Matthew 23:28 so also ye outwardly indeed do appear to men righteous, and within ye are full of hypocrisy and lawlessness. Matthew 23:29 'Woe to you, Scribes and Pharisees, hypocrites! because ye build the sepulchres of the prophets, and adorn the tombs of the righteous, Matthew 23:30 and say, If we had been in the days of our fathers, we would not have been partakers with them in the blood of the prophets. Matthew 23:31 So that ye testify to yourselves, that ye are sons of them who did murder the prophets; Matthew 23:32 and ye—ye fill up the measure of your fathers. Matthew 23:33 'Serpents! brood of vipers! how may ye escape from the judgment of the gehenna?
and prophesieth of the destruction of Jerusalem.


The Life of the Buddha website presents two types of materials: (1) the narrative mural panels that appear in the image window, initially at the left; and (2) the various texts associated with the murals, initially at the right. The latter include the literary narrative titled Sun of Faith (in English and Tibetan), the Painting Manual (in English and Tibetan), the mural inscriptions (in English and Tibetan), and citations to the story's sources in the Tibetan canonical literature.
The website likewise provides two ways to approach these materials. You can begin by selecting a text, such as a chapter from the Sun of Faith, which will highlight the relevant part of the mural in the center of the image window. The mural will then "follow along" as you read and click through the text. You can also begin by exploring the mural, panning and zooming the image window, and clicking links in the pop-up windows that appear as the cursor moves across the window.
You can open multiple text windows simultaneously, such as the English and Tibetan versions of the Sun of Faith, and rearrange them in various configurations.
The easiest way to begin reading the Life of the Buddha is to select a chapter from the Table of Contents on the left. You can then close the ToC tray and begin reading the text. Click on the first line of text you want to read. Then navigate down/up by using the arrow keys on your keypad. As you move through the text, the associated part of the mural will appear in the center of the image window.
The Life of the Buddha project includes three different texts: (1) the literary narrative of the Buddha's life story titled the Sun of Faith; (2) the Painting Manual, which gives instructions on how to visually depict the literary narrative; and (3) the inscriptions included on the mural surface. All three are available in both the original Tibetan and English translation.
The Sun of Faith is divided into chapters, and each chapter is further divided into smaller scenes. In the text, these are marked by black bars (for chapters) and gray bars (for scenes), with corresponding numbers. Chapters and scenes are also outlined on the mural.
The simplest way to navigate the Sun of Faith is to select a chapter from the Table of Contents window at the left. Clicking a chapter opens a text window at the right with the Sun of Faith and the corresponding part of the mural in the image window.
You can select the desired text and language from the dropdown menu at the top of the text window.
Mural images appear in the image window, initially at the left side of the screen.
You can zoom and pan across the mural image in several ways. Zoom in and out of the mural image by clicking the "+" and "–" buttons at the lower right corner of the image window. Double clicking on the image will zoom in. The scroll feature of your mouse will also zoom in and out.
Pan across, up, and down an image by clicking the arrow keys at the lower right corner of the image window. Clicking the home button at the center returns the image to its original size. Clicking and dragging the cursor over the image will also pan in any direction.
You can select a different mural panel from the "canvas list" at the bottom of the image window. The canvas list can be open and closed by clicking the "…" icon at the bottom of the image window. Once the gallery is open, you can select the desired mural panel.
Moving the cursor over the mural image will highlight the associated chapter or scene and open a pop-up window. You can find related texts by clicking on the link(s) in the pop-up window. The associated text will appear in a window to the right of the image.
You can lighten the images by clicking the image adjustment icon (three sliders) at the upper left of the image window. Click the sun icon and move the slider up or down as needed.
To add a text window, click the "plus" (+) symbol at the upper right hand corner of any currently visible text window.
To remove a text window, click the "x" next to the word "annotations", located to the upper right of any text window.
To resize a text window, place the cursor between windows until a double-arrow appears; drag to resize.
To move a text window, click the "Annotations" tab at the top and drag to the desired locations. Text windows may be placed on left/right side or the top/bottom of the screen, in any combination. To combine multiple windows together as tabs within a single frame, drag the "Annotations" tab of one window to the tab bar of any other window.
To view the image window in full-screen mode, click the double-arrow icon in the upper right corner of the image window. Click the icon again to return to normal view mode.
It is possible to search for key terms such as proper names, places, and other text strings. From the homepage: http://lifeofthebuddha.org, enter a term into the search box in the upper right header and press return/enter. This will result in a list of all instances in which the term appears, across all texts, together with thumbnails of the associated image. It is then possible to filter results by text source, panel, chapter, or scene.


Lychee Wintour by Okami is just like Lychee Lauren, but with a shot of menthol! A harmonious mix of white peach, lychee tea, and a cool finish. Two delicate and sweet fruits combined to make your taste buds scream!


text:
Navi Is...
The Dead Travellers
My Flatmate is a Monster
(on) WHATIPU
Precious Little
Balls Papakura
The Snot-Gobbler
Gruesome Playground Injuries
Make 'Em Think
As the lights faded to black they just sat there, still - it was a really special moment, because until that moment I didn't know that THAT was what I was trying to achieve.
The final night of Balls at my hometown theater was nothing less than an emotional roller coaster. The energy of the final night, the feeling of relief that we had pulled it off, the sadness that it was finishing... The Lads (and the lady) really did the show credit and brought it to life and I was so proud of all of us.
But the best moment for me actually came after the final scene. Three of the people who sat next to me (two of which I knew) just sat there, they didn't move; even after everyone had exited into the foyer, they were still in their seats. I dared not move (as I was sitting pretty much in the middle), but then finally one of them spoke, it was actually the person I didn't know and it was question after question, How did you come up with that? How long did it take you to write? Each answer usually prompting another question.
Now look, I don't want to sound pretentious. I'm just a kiwi boy from South Auckland - but the fact that something I wrote made somebody sit there stunned, thinking over and over about what they had just seen was pretty cool; in fact it was awesome and until that moment I didn't even know that that was what I was trying to achieve. But of course, I wanted to create a story that not only entertains but also makes you think. I love engaging with stories myself, and It was such a privilege to give that experience to others.
So now it's all over, what happens next? I know I would love to take the show on the road, tour it around Aotearoa because Balls is more than a South Auckland story, it is a New Zealand story and it is (for better and for worse) part of our entire country's culture. In a recent New Zealand Rugby investigation 36 cases of misconduct were sited in the past four years. These included: "incidents involving inappropriate sexual behaviour, violent behaviour towards team members or coaches, drug and alcohol offenses and homophobic slurs." These sitings show that "Balls" hit the nail on the head with it's interpretation of this part of who we are, and I'm sorry, but it's ugly! I love rugby, I've said that continually throughout that process - growing up me and my Dad really bonded over this beautiful game, and he taught me everything I know about it - but he also taught me to be kind, honest and real.
-Joshua Baty
Link to the New Zealand Rugby Investigation:
http://www.radionz.co.nz/news/sport/338899/nz-rugby-culture-review-findings-released
Making Navi History!
Last evening (the 6th of Sep) we opened our play, Balls, for the second time in two years. And what an opening it was! I felt such gratitude and pride as I watched Josh lock up the Off-Broadway theatre a long while after the last member of the audience has departed.
Balls, in the world of Navi, is a "Toddler Project." In 2016 it became the second company created piece, and this year is has officially become the first show in what will eventually be our Navi "Catalogue." Over the past two months Josh has taken the first full length play that he has written and made it his first show to direct, and I think for a first time Director (with no official training in the art of Directing) he did a damn fine job.
Last night was also history making for Navi, as we had the largest opening night audience in our young Collaborative's life. The energy in the space was delicious and invigorating. I was thrilled to hear the roar of laughter and the sharp intakes of breath as the show moved from one beat to another.
As our Navi Team sat in the theatre afterwards I felt so much love for each of our members. Each member of Navi has worked hard to get Balls to Papakura and what's more we did it while loving and supporting one another through all of the inevitable ups and downs of a show process. We still don't have everything down perfectly, but we are growing. I can see our growth and it that makes me feel joyful and inspired to keep going and revealing what our Collab, our creative family, can do
-Dawn


text:
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Lucy's story – the positive impact of care
Lucy and Stuart Bradley understand the positive impact that care can make, both within the communities where they live and within their own family.
The couple have dedicated their lives to helping others. Lucy worked in a nursing role in a remote area of Irian Jaya (now West Papua) and Stuart served as a pastor for many years in the RAAF. As Christian missionaries, they have also cared for their communities in New Guinea, Vietnam, Nigeria, and London. The Bradleys raised their own two children and fostered two Vietnamese children.
In 2003 the Bradleys took up an opportunity to live and work at the Christian Convention Centre on Tamborine Mountain. For seven years Stuart continued his pastoral work and maintained the buildings and surrounding acreage, while Lucy looked after the guests and visitors at the Centre.
In 2010 Lucy was diagnosed with Multiple Sclerosis. As retirement approached, the Bradleys left the Centre and moved to Brisbane to enjoy a quieter pace of life including gardening and gentle walking which suited Lucy.
In 2018, Lucy began to experience a decline in her physical health and cognition, so the couple contacted Suncare to investigate what help was available. Following a visit from the Aged Care Assessment Team, it was confirmed Lucy was eligible to receive the Short-Term Restorative Care (STRC) Program, and within weeks she had a team of Allied Health professionals helping her to work towards her wellbeing goals.
The Short-Term Restorative Care Program was delivered in the Bradley's home over an eight-week period and included podiatry, physiotherapy and psychology services. Lucy was also introduced to some brain training games from her occupational therapist, which both Lucy and Stewart found very beneficial.
Using some of Lucy's photographs as inspiration for the game, the occupational therapist made two copies of several photos and laminated them. The laminated photocopies are placed face down on a table so Lucy can turn them over, two at a time, to try and find a matching pair.
"The advantage of this game is twofold; it is a memory game for Lucy, and it also invokes memories associated with the photos," said Stewart. 'The photos bring back memories of family, friends and the places we've visited. It's been such a good idea.'
Lucy and Stewart are so pleased with the support the STRC program has provided to Lucy and they look forward to continuing with the exercises and brain training games they received during the eight-week program.
If you or someone you love could benefit from a Short-Term Restorative Care program or would like to talk about your health and wellbeing needs, please contact the Suncare Customer Service Team on 1800 786 227.
How do I access services?
We understand that beginning your journey into home care services can be a daunting path, so our friendly team are here to guide you through and help you every step of the way, our knowledgeable team will be able to answer your every question.
What kind of services does Suncare provide?
Once you have been assessed by My Aged Care and allocated an appropriate program or package you can discuss with Suncare the most appropriate services that you would like to receive.
Can you provide services in my area?
Suncare provides home care services throughout Southeast and Central Queensland and we have offices in North Lakes, Sunshine Coast, Gympie, Wide Bay and Rockhampton.
Our staff connect to communities from the regions all around these areas to ensure the best care is easily accessible.
I have a Home Care Package, can I use Suncare's services?
Yes, Suncare can be your service provider if you have been allocated a Home Care Package. We will work with you to identify a total package of care and services to meet your needs so you can continue to live a more active and independent life. If you are an existing customer of Suncare, you are familiar with of our level of commitment but may not be aware of the complete package of services we provide.
Government funding extended
The 2019-20 Federal Budget announced that funding for the Commonwealth Home Support Programme will be extended from 1 July 2020 to 30 June 2022. The Commonwealth Home Support Programme is designed for people who are living independently but require a...
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Why I prefer a 5 minute TICK chart instead of a 1minute TICK. Explains some simple but yet very powerful TICK hook and fade strategies.
Great video. Good way of profiting from the up trend. My only question is that when illustrating the tick hooks you put the crosshair right on the low of the tick hook but surely in real time you would only see it was a hook at the close of the next period? For example on that first tick hook you showed you said you may have been stopped out but the tick only actually hooked in the following period - which would have been the perfect entry (corresponding to the bullish hammer on the price chart).
Yep youre right. The entry would be a little after the TICK hook formation, which makes alot more trades profitable.
Very nice video. I like the simplicity of the strategy. It's an uptrending market but the evidence of the hooks and extremes is a very solid set up.
Hello, Thank you for sharing the video. However the link is now broken.