text:
\section{Introduction}
\label{sec:intro}
Cygnus region, located between $70^o<l<80^o$
is a region of recent star formation activity in the
Milky Way and is rich in massive early type stars concentrated in OB
associations. The presence of nebulosity
and massive stars indicate that the stars have been forming till
very recently and the young clusters found here are the result of the recent
star formation event. Though the above fact is known, what is not known is that
when this star formation process started and how it proceeded in the region.
Thus the aim of the paper is to understand the star formation timescale
in this complex, using the recently formed young open clusters.

Though one assumes that all the stars in a cluster have the same age,
this assumption is not valid when the candidate cluster is very young.
In the case of young clusters ($\le$ 10 Myr), there is a chance
for a spread in the age of the stars, depending on the duration
of star formation. An estimation of this formation time-scale in the
clusters formed in a star forming complex, will indicate the duration
of star formation and its direction of propagation within the complex.
In principle, duration of star formation is defined as the
difference between the
ages of the oldest and the youngest star formed in the cluster.
In practice, the age of the oldest star is assumed as the age of that star
which is about to turn-off from the main-sequence (MS) (turn-off age) and
the age of the youngest star is the age of the youngest pre-MS star (turn-on age).
The turn-off age of many clusters are known, but the turn-on age
is not known for most of the clusters. The estimation of turn-on age
requires the identification of pre-MS stars in the cluster.
Hence the duration of star formation in
young star clusters is not clearly understood.
This quantity cannot be
estimated for older clusters where all the stars have reached the MS.
The star clusters  studied here are
Berkeley 86, NGC 6910, IC 4996, Berkeley 87 and Biurakan 2.
We aim to combine the ages and the star
formation duration in these clusters to understand how the star formation
proceeded in the Cygnus region.

A number of stars are known to show H$_\alpha$ emission in this region.
The photometric analysis of the clusters suggested the possible presence of a few
emission line stars. As a followup, we searched, identified and studied these stars.
Since the estimation of cluster parameters will help in identifying the
ages and spectral types of these stars, their emission properties
can be linked to their evolutionary status.
Early type emission stars are broadly classified as Classical Be (CBe) stars and
Herbig Ae/Be (HAeBe) stars, which belong to intermediate mass pre-MS category.
CBe stars are fast rotators whose circumstellar disk is formed through
decretion mechanism (wind/outflow) (Porter \& Rivinius 2003). HAeBe stars are
found to possess a natal accretion disk which is a remnant of star formation
(Hillenbrand et al. 1992). The emission is found to come from this equatorial disk as
recombination radiation, mainly in Balmer lines like H$_\alpha$ and H$_\beta$.
We have used slitless spectroscopy to search for these emission stars. Emission stars
are found to show an IR excess, which is a combination of free-electron excess
and dust excess. We combine the parent cluster parameters and the spectral properties
of emission stars, and try to classify them. Fabregat \& Torrejon (2000)
suggested that emission stars found in clusters younger than 10 Myr belong to the
HBe type and CBe stars are found only in clusters older than 10 Myr.
On the other hand, the HAeBe phenomenon is known to last
only for a few Myr (Hillenbrand et al. 1992). Thus
it will be interesting to identify and classify emission stars in clusters
younger than 10 Myr.

In the following section, we present the data used and discuss the analysis
of the photometric data. Section 3 deals with the results obtained for the 5 clusters.
In section 4, we present the spectra  and discuss the emission line stars.
A discussion
of the star formation in Cygnus region is presented in section 5. The conclusions drawn from this
study are listed in section 6.

\section {Observations and Analysis}
The photometric data of clusters in the UBV
optical pass bands are taken from WEBDA
(http://obswww.unige.ch/webda), a website devoted for star clusters.
The photometric data in the near-infrared (NIR) in J, H, K
pass bands are taken from 2MASS data
(http://www.ipac.caltech.edu/2mass/overview/access.html).
The reddening and extinction towards the clusters are already available in WEBDA.
The ZAMS data for distance determination were taken from Schmidt-Kaler (1982).
The pre-MS isochrones for estimating the pre-MS age of the cluster are
taken from Siess et al. (2000)

\subsection{Identification of pre-MS stars}
In the optical colour-magnitude diagram (CMD), both pre-MS stars and
field stars occupy the same region (right side of the MS) and
we cannot distinguish between the two in the CMD.
Spectroscopic identification of pre-MS stars could be done at the
brighter end, but is inefficient for fainter stars.
In the case of pre-MS stars, the dust grains
in the circumstellar disk absorb a fraction of visible or ultraviolet photons
emitted by the central star, heating it to a higher temperature.
The disk re-radiates the absorbed energy in infra-red wavelengths.
Thus the presence of NIR excess is used to distinguish between the pre-MS stars and
field stars in the optical CMD.
Thus, pre-MS stars can be identified using near-infrared (NIR) photometry.
By cross-correlating optical and infrared images of the cluster field,
the J, H, K magnitudes of optically identified stars were found.
We used the
(J$-$H) vs (H$-$K) NIR colour-colour diagram
to identify stars with NIR excess and to determine their nature (Subramaniam et al. 2005).
The intrinsic location of un-reddened giants and MS stars,
and the normal reddening vector,
which limits the reddening due to normal interstellar dust are used to distinguish
various types of stars with NIR excess.
By relating their position in the NIR colour-colour diagram with the general
location of HAeBe and CBe stars, we identify candidate stars belonging to
the above classes.

\subsection{Estimation of turn-on age}
The stellar magnitudes were corrected for reddening and extinction.
Though the distance to the clusters have already been estimated, we
re-estimated the distance, which in most cases turned out to be similar to the
already estimated value.
The dereddened and extinction corrected CMD is fitted with ZAMS to estimate
the distance modulus (DM).
The turn-off age of the clusters have already been estimated and we adopt these values.

In the NIR colour-colour diagram, stars which have NIR excess were identified.
These stars were plotted
on the optical CMD, as candidate pre-MS stars (indicated by a different symbol).
Pre-MS isochrones of different ages from Siess et al. (2000)
were fitted to these stars on the CMD.
The presence of pre-MS stars in more than one isochrone shows
that the pre-MS stars have a range in age, which in turn would indicate that
the stars were formed over a time-scale.
The age of the youngest pre-MS star would be the turn-on age of the cluster.

\section{Results}

\subsection{IC 4996}
IC 4996 is located ($RA=20^h14^m24^s$, $Dec=+37^o29'$, $l=75.36^o,b=1.31^o$)
in the direction of the Cygnus and is part of a star forming region.
An IRAS map of the region (Lozinskaya $\&$ Repin 1990) shows
the presence of a dusty shell around the cluster. Zwintz and Weiss (2006) have performed
time series CCD photometry in Johnson B and V filters to find 40 stars to lie in the
classical instability strip of the 113 stars analysed in the cluster. They have discovered
two \ delta Scuti-like pre-MS stars in the cluster. The parameters obtained by
Delgado et.al (1998) for the cluster are $E(B-V)$=0.71 $\pm$ 0.08 mag,
DM = 11.9 mag and age of 7.5 $\pm$ 3Myr. They suggested a
number of pre-MS
stars in the cluster, which are located at 0.5 and 1 magnitude above the MS
in the V vs (B$-$V) CMD, around the location of spectral types A-F.
Delgado et.al (1999) estimated the spectral types and heliocentric radial velocities
for 16 stars in the cluster and the mean radial velocity was found to be
$-$12 $\pm$ 5 kms$^{-1}$.
Vansevicius et.al (1996) estimated the distance and age of the cluster to be 1620 pc
and 9 Myr respectively, using BVRI CCD photometry. Pietrzynski (1996) performed variability
studies on the cluster and found an RR Lyrae type variable
and another eclipsing system. According to WEBDA, cluster contains two
B type emission stars.\\

We used the optical data of Delgado et al. (1998), available from WEBDA.
From the field of the cluster, 84 optically identified stars were
found to have counterparts in the 2MASS data. We combined the
V, (B$-$V), (U$-$B) (taken from WEBDA) and  J, H, K (taken from 2MASS)
magnitudes for 84 stars.
From the NIR color-color diagram (figure 1), 22 members are found
to be located below the
reddening vector. Among them, 15 could be considered
to be candidate pre-MS stars and these are shown as dots with open circles
around them. Star numbered 23 is found to have H$_\alpha$
emission and shown as labeled filled circle.
The MS and the giant star locations in the CMD are shown
(Bessell \& Brett 1988). The location of T-Tauri stars is shown as the dashed straight
line (Meyer et al. 1997). The location of Be stars is taken from Dougherty et al. (1994)
and the location HAeBe stars is taken from Hernandez et al. (2005).
The diagram on the left is not corrected for the reddening towards the cluster, whereas
the figure on the right is corrected for the reddening.
The reddening value as estimated from the ZAMS fitting is used for dereddening.
The relation from Bessell \& Brett (1988)
is used for converting reddening in the optical to NIR.
This could also arise due to differential reddening.
Star 23 is likely to be a CBe candidate.

The identified stars are reddening and extinction
corrected by taking E(B$-$V) as 0.7 mag and R$_v$ as 3.1.
The DM is estimated as 11.8 $\pm$ 0.2.
and the distance as 2291 $\pm$ 225 pc, which is similar to that estimated
by Delgado et al. (1998). The turn-off age of
the cluster is 7.5 $\pm$ 3 Myr (Delgado et.al 1998).
Pre-MS isochrones for ages 0.25, 0.5, 1, 3, 5 and 7 Myrs are
plotted as shown in the Figure 2.
The presence of pre-MS stars on or near all the pre-MS isochrones shows that
the stars have been forming continuously for the last 7 Myr.
Also, the presence of pre-MS stars near the tip of the MS indicates that
some of the high mass stars could be very young and the star formation stopped very recently.
Thus, the duration of star formation is similar to the age of the cluster, i.e.,
$\sim$ 7 Myr. The H$_\alpha$ emission star is located slightly to the
right of the MS  and there are a few candidate pre-MS stars located nearby.
Therefore, this star could either be a MS CBe star or a pre-MS HBe star.
If it is a pre-MS
star, then the isochrones indicate its age to be between 0.5 -- 0.25 Myr.
If it is a CBe star, then its age is $\le$ 7 Myr.

To study the distribution of pre-MS stars within the cluster, we compared the location of
pre-MS stars and normal stars, as shown in Figure 3.
Pre-MS stars are shown as filled circles and normal stars as open circles. The
emission line star (23) is also labeled.
The pre-MS stars are found to be located relatively closer to the center
of the cluster when compared to the normal stars.

\subsection{NGC 6910}
NGC 6910
($RA=20^h21^m18^s$, $Dec=40^o 37'$, $l=78^o .66, b=2^o .03$)
is a young open cluster
located in the Cygnus region and is a part of the Cygnus OB9 association.
This cluster is located in the
core of the star forming region, 2 Cygni. It is surrounded by a series
of gaseous emission nebulae which resemble Barnard's loop in the Orion.
From UBV CCD observations down to V=18 mag for 206 stars in the
cluster, Delgado et.al (2000)
found eleven pre-MS stars of spectral type A to G.
They estimated the cluster parameters to be
$E{(B-V)}$ = 1.02 $\pm$ 0.13, DM = 11.2 $\pm$0.2 and
age = 6.5 $\pm$ 3 Myrs. Kolaczkowski et al. (2004) found four beta Cep-type
stars along with three
H$_\alpha$ emission stars, while searching for variable stars in the
cluster. They  suggest a
possibility of finding a large number of beta Cep stars in
the cluster due to
higher metallicity of the cluster. Using $VI_c$ and $H_\alpha$ photometry they have
determined an age of 6 $\pm$ 2 Myr, DM of 11.0 $\pm$ 0.3 mag and
an $E(B-V)$ value varying from 1.0 to 1.4 magnitude.
Shevchenko et al. (1991) studied the cluster using UBVR photoelectric
photometry. From the photometry of 132 stars,
they found the HAeBe stars BD +40 41 24 and BD +41 37 31 to be associated with it.
The extinction is
high in the region with a value of $E(B-V)$ = 1.2 mag and the value of
R = 3.42 $\pm$ 0.09.
Using intermediate-band photoelectric photometry for
16 cluster members, Crawford et.al (1977)
obtained a reddening value of $E{(b-y)}$=0.75 mag and a DM of 10.5 mag.
They found that a type Ia super giant star
of $M_v$ = -6.9 to be associated with the cluster. According to WEBDA there is no
emission star in the cluster.\\

The U, B$-$V, U$-$B values of 148 stars are taken from WEBDA (Delgado et al. 2000).
The J, H, K values of these stars are taken from 2MASS by cross-correlating
optical and IR images. NIR colour-colour diagram is plotted as shown in Figure 4.
47 stars were found to be located below the reddening vector.
Out of them, 23 members were found to have relatively large IR excess and were considered as
candidate pre-MS stars. Stars, 26 and 181 do not have CCD photometry, we have
used the UBV photographic photometry of Hoag et al. (1961). These stars show
$H_\alpha$ emission and are shown as dark filled circles.  After dereddening,
star 181 can be found very close to the CBe location, indicating its CBe nature.

The reddening and extinction
corrections are done by assuming E(B$-$V) as 0.97 mag and $R_v$ as 3.1.
ZAMS fitting is done as shown in Figure 5, the DM is estimated as
11.8$\pm$0.2 mag and the distance as 2291$\pm$225 pc. The
turn-off age of the cluster is 6.5$\pm$3 Myr (Delgado et al. 2000).
The pre-MS isochrones for 0.5, 1, 2, 3, 5, 7.5 and 10 Myrs are overlaid
on the CMD.
The presence of pre-MS stars
with these ages shows that star formation processes are occurring
in the cluster continuously. More number of stars are formed
in the early stages and continuing up to 3 Myr.
After that the star formation seems to have continued
 but in a slower rate, till 0.5 Myr. We find that a few pre-MS stars are as old as
10 Myr. Also for this cluster, we get the duration of star formation
as the cluster age itself $\sim$ 7 Myr, though there is an indication that
the star formation started 10 Myr ago.
The H$_\alpha$ emission star 181 is found to be
located near the 0.5 Myr isochrone, indicating that this could also be a candidate
HBe star. The star 26 is located to the left of the MS, hence we do not discuss
the nature of this star based on the photometry. The peculiar location may be due to
two reasons - we used the photographic data for these two stars and there
may be some error in the data of this star, or, the reddening is very different for this star.
If these two stars belong to the CBe class, then these stars are $\le$ 7 Myr old.

The pre-MS
stars are shown separately as dark circles and normal
stars are shown as open circles, as
in Figure 6. We find that the pre-MS stars are scattered throughout the face
of the cluster. The emission stars 26 and 181 are located very close to each other.

\subsection{Berkeley 87}

       The open cluster, Berkeley 87
(Dolidze 7,$ RA=20^h21^m42^s, Dec=37^o.22$),
 located at $l=75^o .71, b=+0^o .31$ is a
 sparse grouping of early-type stars lying in a heavily
 obscured region in the Cygnus. Turner \& Forbes (1982)
derived a distance of 946 $\pm$ 26 pc and an age of 1-2 Myr
for the cluster from UBV photometry of 105 stars. The age as
reported in WEBDA is 14 Myr.
The distance was estimated to be 0.9 kpc from the interstellar
line depth of the cluster members (Polcaro et al. 1989).
It is part of the star formation region ON 2, which harbours many
compact HII regions, strong OH masers and CO and ammonia molecular clouds.
Diffuse emission in CIV 5802-12 A doublet and X-ray emission in 2-6 keV
range has been detected in the cluster,
which is interpreted as due to the interaction of the strong wind from a
Wolf Rayet star (ST 3) of
velocity 5200 kms$^{-1}$ with the cluster members. A high energy
 Gamma ray source 2CG 075+00 ($\le$100 Mev)
has been found to be associated with this cluster. Be 87 contains a
peculiar emission-line B super giant HDE 229059 (Hiltner 1956),
two faint objects (VES 203 and VES 204) which show
H$_\alpha$ in emission (Coyne et.al 1975), the red super giant
BD +37 39 03 and the faint
variable star V439 Cygni. According to WEBDA the cluster contains 5
B type emission stars.\\

The optical data of 94 stars (Turner \& Forbes 1982) were combined with
the 2MASS data.
 19 stars were identified to have possible NIR excess from the NIR colour-colour
diagram (figure 7). Out of them, 13 members having relatively
 higher (H$-$K) magnitudes were grouped as candidate pre-MS stars. Stars 9, 15, 38
 and 68 (Turner \& Forbes 1982) are stars with H$_\alpha$ emission,
shown as filled circles.
 Star 38 and 15 occupy the HAeBe location, after the reddening correction. Stars
9 and 68 are likely to be CBe stars. There is significant differential
reddening in this cluster, as discussed below. Therefore, the above classification
should be taken with some caution.

 In the NIR colour-colour diagram, many stars are found outside the
 reddening vector. Some stars are more reddened than others
 i.e., there is a variation of  reddening in different parts of
 cluster field. All cluster members do not have the same $E(B-V)$ value.
 Color correction and extinction correction are done by choosing
$E(B-V)$ as 0.45 for stars
 having (H$-$K) value less than 0.1 and as 1.35 for stars having (H$-$K)
 value higher than 0.1 along with $R_v$=3.1. The variation in $E(B-V)$
 gives an indication of the non-uniform distribution of interstellar material
within the cluster. The resulting CMD is shown in figure 8.
The wide MS in the CMD is an indication of significant differential reddening
across the cluster.
The dereddening in the NIR is done using the lower value of the two reddening
values.

 ZAMS fitting estimated the DM
 to be 10.8 $\pm$ 0.2 mag. The distance estimated is 1445 $\pm$ 145 pc, higher
than the value estimated by Turner \& Forbes (1982).
 The pre-MS isochrones for the ages 0.15, 0.2, 0.25, 0.5, 1, 1.5 and 2 Myrs are
 plotted on the CMD (shown in Figure 8). Most of the pre-MS stars are located
 in isochrones of ages ranging from 0.15 to 2 Myr. Therefore, the turn-on
age of the cluster is less than 1 Myr, which is consistent with the
recent star formation activity in the cluster vicinity. This recent star
formation activity is likely to have started 2 Myr back, as indicated by the
age of the pre-MS stars.
 The cluster has a turn-off age of 14 Myr, as indicated in WEBDA. On the
other hand, the age of 2 Myr as estimated by Turner \& Forbes (1982), is in good agreement
with our estimation of the starting time of the star formation. Therefore, this may be a  very young
cluster with a turn off age of 2 Myr. Therefore, we consider the turn-off age
of Be 87 as 2 Myr. The emission line stars in this cluster are very young.
If they are HAeBe stars, then they are as young as 0.15 Myr. If they
are CBe stars, then they are $\le$ 2 Myr old. Thus, if these stars are CBe stars,
these might be one of the very young CBe stars known.

The location of pre-MS stars in the field of the cluster is shown in figure 9.
It can be seen that there is a clustering
of pre-MS stars as well as the emission stars towards
the central region of the cluster.

\subsection{Biurakan 2}
       The galactic cluster, Biurakan 2, is
 ($RA=20^h09^m12^s,
 Dec=35^o.29$,  $l=72^o.751, b=1^o.345$) also located
 in the vicinity of the association, Cygnus OB-1.
The cluster was studied by Dupuy and Zukauskas (1976)
using photoelectric and photographic photometry.
They estimated
an average value of E(B$-$V)=1.39$\pm$.09 towards the cluster,
DM as 10.8$\pm$0.2 mag, which corresponds to a distance of 1445$\pm$133 pc
and age $\le$10 Myr. According to WEBDA there is no Be star in the cluster.\\

By cross-correlating the optical (Dupuy \& Zukauskas 1976) and NIR data of
the cluster field, 114 stars were identified to have both data.
NIR colour-colour diagram is plotted as shown in Figure 10.
 33 stars were found to be
 located below the reddening vector and 15 stars having
 higher (H$-$K) were grouped as candidate pre-MS stars. No star with
 H$_\alpha$ emission is observed in this cluster.

 Assuming $E{(B-V)}$ as 0.45 mag and $R_v$ as 3.1, colour  correction
 and extinction correction were done and the resulting CMD
 is shown in Figure 11.
We re-estimated the DM as  11.2 $\pm$ 0.2 mag. The distance
obtained is 1737.8 $\pm$ 175 pc.
 The pre-MS isochrones for the ages 0.5, 1, 1.5, 2, 3 and 5 Myrs are plotted.
 The presence of pre-MS stars in these isochrones shows that the pre-MS stars
have an age range of 0.5-5 Myr. Most of the pre-MS stars are younger than 2 Myr
and only four stars were found to be older than 5 Myr.
This indicates that the star formation started 5 Myr back, but was very active for the
last 2 Myr.
   The turn-off age of the cluster obtained by the previous study
is 10 Myr  or less (Dupuy et.al 1976). The turn-off age estimation is difficult and
inaccurate due to the absence of evolved stars. It is quite likely that the turn-off age
of the cluster is 5 Myr, which is the time when the star formation started.
The turn on age is less than 1 Myr. Thus the duration of star formation in this cluster
is about 5 Myr.

 We compared the location of pre-MS stars in the cluster field, as shown
in figure 12. It can be seen that the pre-MS stars are distributed across
the cluster field and do not show any central concentration.

 \subsection{Berkeley 86}
Berkeley 86, a young open cluster, is one of the three nuclei of
the OB association Cyg OB 1.
The core of this cluster is located at $ l=76^o.7, b=1^o.3 $.
Optical photometry was carried out in UBVRI bands by Deeg \& Ninkov (1996) and
Massey et al. (1995).
They found the cluster to be a young one with a turn-off age of 5 Myr, reddening of 1 mag
and an initial
mass function close to the Salpeter value. Be 86 hosts the famous eclipsing binary
system V444 Cygni (Forbes 1991).
Stromgren photometry was obtained by Delgado et al. (1997) down to V=19 mag, from which
they estimated an age of 8.5 Myr and a distance of 1659 pc.
Forbes (1981) found Be 86 to lie at a distance of 1.72$\pm$0.20 kpc with a
reddening of E(B$-$V)=0.96$\pm$0.07 mag.
The cluster is located in the Orion spiral feature and is a possible member
of the Cygnus OB 1 association at 1.8 kpc.
An age of 6 Myr was estimated based on the earliest spectral type of O9.
Vallenari et al. (1999) studied about 2000 stars in the
field of Berkeley 86 down to K $\sim$ 16.5 mag
using near-infrared photometry in J and K bands. They have found a
number of pre-MS stars from
(V$-$I) vs (I$-$K) plot and J vs (V$-$J) diagram. They do not estimate the
ages of their candidate pre-MS stars. According to WEBDA cluster contains
3 Be stars.\\

From the field of Be 86 about 191 stars are identified with
V, (B$-$V), (U$-$B), J, H, K magnitudes. Optical data is taken from
WEBDA (Deeg \& Ninkov 1996). NIR colour-colour diagram is
plotted for the identified stars as shown in Figure 13.
36 stars are
found to be located below the reddening vector, showing
IR excess. 27 stars are found to have more
IR excess (large (H$-$K) magnitude) and could be
candidate pre-MS stars. Three more stars are located
below the reddening vector (not shown in the figure) with
very large (H$-$K) value. These stars are located in HAeBe
location, could be probable HAeBe stars.
The stars 9 and 26 (Forbes 1981) for which H$_\alpha$ emission was
observed are shown as filled and labeled circles. In the reddening
corrected figure (right panel), these stars occupy the CBe location.

For the identified stars reddening and extinction
correction are done by assuming $E(B-V)$ as 0.95 mag and $R_v$ as 3.1.
The resulting CMD is shown in Figure 14.
We re-estimated the distance as 1585$\pm$160pc.
 In the CMD,  many stars fainter than $V_0$ = 14 mag and having
IR excess are located to the left of ZAMS. These may be field stars or stars with
different reddening.
 The turn-off age of the cluster is 6 Myr (Forbes et al. 1992).
 Pre-MS isochrones of ages 0.25, 0.5, 5, 7.5 and 10 Myrs are
 shown. The pre-MS stars are distributed in two age groups.
The younger group is found to be younger than 1 Myr, while the older group
is as old as or older than 5 -- 7 Myr. It is quite likely that the star formation
in this region started around 5 Myr and had a relatively low level star formation
till 1 Myr. The cluster region has experienced vigorous star formation in the last 1 Myr.
The duration of star formation is about 5 Myr, which is similar to the cluster, Biurakan 2.
Star 9 lies on the 0.25 Myr pre-MS isochrone and 26 is located on the 0.5 Myr isochrone.
Thus these stars are could be younger than 1 Myr, which makes them as candidate HAeBe stars.
Otherwise, these stars could be 5 Myr old or slightly older, which would make them as
candidate CBe stars.
The Pre-MS stars are found to be distributed throughout the cluster field, as shown in Figure 15.
\section{Spectroscopic detection of emission line stars}

\begin{table}
\caption{Log of observations of Individual Clusters in the slit-less mode}
\vspace{0.5cm}
\centering
\begin{tabular}{ccccccc}
\hline
Date of & Cluster & Filter/ & Exposure & RA & Dec\\
observation &    & Grism  & Time   & hh:mm:ss & deg:mm:ss\\
\hline
30-10-2003 & IC 4996 & R & 5 & 20:16:30 & +37:38:00 \\
           &         & R/Gr5 & 60 & & \\
           &         & R/Gr5 & 300 & & \\
22-11-2004 & NGC 6910 & R & 5 & 20:23:12 & +40:46:42 \\
           &          & R/Gr5 & 60 & & \\
           &          & R/Gr5 & 180 & & \\
           & NGC 6910 & R & 10 & & \\
           &          & R/Gr5 & 600 & & \\
15-07-2005 & NGC 6910 & R & 10 & & \\
           &          & R/Gr5 & 600 & & \\
22-11-2004 & Berkeley 87 & R & 5 & 20:21:42 & +37:22:00 \\
           &             & R/Gr5 & 120 & & \\
           &             & R/Gr5 & 480 & & \\
15-07-2005 & Berkeley 87 & R & 10 & & \\
           &             & R/Gr5 & 900 & & \\
21-07-2006 & Berkeley 87 & R & 10 & & \\
           &             & R/Gr5 & 900 & & \\
27-06-2005 & Berkeley 86 & R & 10 & 20:20:24 & +38:42:00 \\
           &             & R/Gr5 & 600 & & \\
08-06-2004 & Berkeley 86 & R & 30 & & \\
           &             & R/Gr5 & 300 & & \\
           &             & R/Gr5 & 600 & & \\
\hline
\end{tabular}
\end{table}

\begin{table}
\caption{Log of observations of Emission Stars in Clusters (Slit Spectra)}
\vspace{0.5cm}
\centering
\begin{tabular}{ccccccc}
\hline
Date of & Cluster & Star & Grism/ & Exposure & RA & Dec\\
observation &     &      & Slit  & Time   & hh:mm:ss & deg:min:ss\\
\hline
15-06-2005 & IC 4996     & 23 & Gr7/167$\mu$ & 600 & 20:16:29.05 & +37:38:53.9\\
           &             &    & Gr8/167$\mu$ & 600 & & \\
29-07-2005 & NGC 6910    & 26 & Gr7/167$\mu$ & 900 & 20:23:09.76 & +40:45:53.7 \\
           &             &    & Gr8/167$\mu$ & 900 & & \\
           &             & 181 & Gr7/167$\mu$ & 900 & 20:23:11.82 & +40:43:28.8 \\
           &             &     & Gr8/167$\mu$ & 900 & & \\
09-10-2005 & Berkeley 87 & 9 & Gr7/167$\mu$ & 600 & 20:21:29.72 & +37:26:25.1 \\
           &             &   & Gr8/167$\mu$ & 600 & & \\
           &             & 15 & Gr7/167$\mu$ & 900 & 20:21:33.59 & +37:24:51.7 \\
           &             &    & Gr8/167$\mu$ & 900 & & \\
           &             & 38 & Gr7/167$\mu$ & 900 & 20:21:59.9 & +37:26:25.1 \\
           &             &    & Gr8/167$\mu$ & 900 & & \\
           &             & 68 & Gr7/167$\mu$ & 900 & 20:21:28.9 & +37:26:19.9 \\
           &             &    & Gr8/167$\mu$ & 900 & & \\
27-06-2005 & Berkeley 86 & 9 & Gr7/167$\mu$ & 900 & 20:20:10.55 & +38:37:29.8 \\
           &             &   & Gr8/167$\mu$ & 900 & & \\
           &             & 26 & Gr7/167$\mu$ & 900 & 20:20:22.78 & +38:38:12.3 \\
           &             &    & Gr8/167$\mu$ & 900 & & \\
\hline
\end{tabular}
\end{table}

The spectroscopic observations of the emission stars
in clusters have been obtained using  the HFOSC instrument available
with the 2.0m Himalayan Chandra Telescope, located at
HANLE and operated by the Indian Institute of Astrophysics.
Details of the telescope and the instrument are available
at the institute's homepage
(http://www.iia.res.in/). We have used slitless spectroscopic
technique to identify emission stars in a cluster
(Subramaniam et al. 2005). The log of observations of
individual clusters in the slit-less mode is tabulated in Table 1.
Slit spectra for identified emission
stars were taken using Grism 7 (3800\AA-6800\AA) and
167 $\mu$ slit combination in the blue region which
gives an effective resolution of 1330. The spectra in the
red region were taken using Grism 8 (5800\AA-8850\AA) 167 $\mu$
slit setup, which gave an effective resolution of 2190.
The CCD used was a 2 K $\times$ 4 K CCD, where
the central 500 $\times$ 3500 pixels were used for
slit spectroscopy. The log of observations of the identified
emission stars in the slit mode is tabulated in Table 2.
All the observed spectra were wavelength
calibrated and corrected for instrument sensitivity using
IRAF tasks. The spectrophotometric standard, BD
+284211, was observed on corresponding nights and was
used for flux calibration. The resulting flux
calibrated spectra were normalised and continuum fitted
using IRAF tasks. The spectra are shown in figures 16 (blue region)
and 17 (red region). Figure 18 shows the spectra of 4 stars which
show prominent lines in the red end of the optical spectrum.
The spectral
properties of stars in four clusters are discussed below.

NaI lines (5890, 5896\AA), Telluric $O_2$ bands (6867, 7600\AA) and
TiO molecular band (6080-6390\AA) can be seen the spectra of
emission stars in all the clusters.\\

{\bf IC 4996:}
The $H_\alpha$ profile of star 23 (GSC 03151-00898) shows emission in absorption feature
and has OI(8446 \AA) line in emission.\\

{\bf NGC 6910:}
Star 181 has H$_\alpha$
and OI (8446\AA) lines in emission.
The H$_\alpha$ profile is found to show an asymmetry in profile
with a definite V/R ratio.
Star numbered 26 has an emission in absorption feature for H$_\beta$
and H$_\delta$ profiles.

{\bf Be 87:}
Star 9 (B0.5Ve; GSC 02684-00007) shows double peaked
emission for H$_\alpha$ profile
along with H$_\gamma$ and Paschen 14 line in emission. Spectral lines
like OI (8446\AA), Calcium triplet (8498, 8542, 8662\AA) and FeII line
(6384\AA) are seen in emission.
Star 15 has an equivalent width of -3.5 and -32.89 for
H$_\beta$ and H$_\alpha$ profiles respectively, which is the highest among
these 9 emission stars. Intense emission can be seen for
spectral lines like OI (8446, 7771\AA), Paschen lines (P14(8598\AA), P12 (8750\AA)),
 Calcium triplet(8498, 8542, 8662\AA) and FeII lines
(6384, 5316, 7712\AA).
For star 38, (B2IIIe; GSC 02684-00004) only  H$_\alpha$
is seen in emission among the
group of Balmer lines. Faint emission features of OI, FeII(4351, 4620\AA)
and Calcium triplet are seen. He lines (4922, 4471, 4026, 5876, 6678\AA)
are seen in absorption.
For star numbered 68, the H$_\alpha$ profile is seen in double
peaked emission while H$_\beta$
is seen in absorption. The spectrum is more or less featureless with
tentative emission in OI (7772, 8446\AA), Calcium and Paschen lines.\\

{\bf Be 86:}
For the star 9, the H$_\alpha$ profile is found to show a double peak profile with
the red region intense over violet. Balmer lines other than  H$_\alpha$
are in absorption. He lines (4922, 4471, 4026, 5876, 6678\AA)
are seen in absorption.
For the star numbered 26 intense emission can be seen for
spectral lines like OI (7254, 8446\AA),
Paschen lines (P14 (8598\AA), P12 (8750\AA)),
Calcium triplet (8498, 8542, 8662\AA) and FeII lines
(6384, 5316, 7712\AA).
P15 (8545\AA), CaII (8542\AA) lines and P13 (8665\AA),
CaII(8662\AA) are blended due to the low resolution of the
spectrum. In the blue region (3700-4500\AA), Balmer lines other than H$_\alpha$ and
H$_\beta$ (core emission) are seen in absorption.

\subsection{Estimation of stellar and disk properties}
The equivalent width and FWHM of the spectral lines
are estimated from a Gaussian fit, using routines in IRAF.
The FWHM of H$_\alpha$ is corrected for instrument
line width using comparison lines. The rotation
velocity has been calculated using the formula,
$$VSin{\it i}=c*FWHM/(2\lambda_0*(ln2)^{(1/2)})$$

 where
c is the velocity of light, $\lambda_0$ is the
central wavelength of the spectral line.
The rotation velocity estimated using H$_\alpha$
emission line profile gives the rotation velocity
of the disk while that from HeI (4471 \AA) absorption line profile
gives the stellar rotation velocity.
The estimated parameters are tabulated in table 3. Many of the
previous estimates of the spectral types indicate  some
of the emission stars to be giants. We have tried to classify the
stars according to their photometry. The estimated spectral types
are given in table 3. It is evident from the optical CMDs that all the
emission stars are located either on the MS or very close to the  MS.
Also they are not located near the turn-off of the MS, but well below
the tip of the MS. This indicates that
none of the stars are evolving to the giant phase from the MS. Thus,
we consider the luminosity class to be V for all the emission stars.

\begin{table}
\caption{Estimated parameters of 9 emission stars.
The age estimated assuming them
to be pre-MS stars is tabulated in column 3, while the age, assuming them to be MS stars
is tabulated in column 4. The Spectral type is estimated from
the photometry (column 5). The H$_\alpha$ EW is in column 6. The stellar rotation velocity is
estimated from the FWHM of He I (4471 \AA) and disk rotation velocity from H$_\alpha$ are in
columns 7 and 8.
 }
\vspace{0.5cm}
\centering
\begin{tabular}{cccccccc}
\hline
Cluster &  Star &  Age & Age &   Sp. type &
 Eq.width&
 Disk Velocity & Star Velocity \\
 & & (pre-MS)& (MS)& & & kms$^{-1}$ & kms$^{-1}$\\
\hline
 IC 4996 & 23 & 0.5 &7& B2.5 & $-$18.99$\pm$1.13 & 268$\pm$6 & 301$\pm$5 \\
 NGC 6910& 26 & - &7& B2.5 &$ -$9.24$\pm$0.45 & 228$\pm$5 &  234$\pm$6 \\
  & 181 & 0.5 &7& B5 & $-$29.25$\pm$2.09 & 339$\pm$36 & 224$\pm$3 \\
 Be 87 & 9 & 0.2 &2& B1.5 & $-$22.87$\pm$1.22 & 352$\pm$8 & 266$\pm$7 \\
 & 15 & 0.1 &2& B1.5 & $-$32.89$\pm$1.87 & 196$\pm$3 & 264$\pm$3 \\
 & 38 & 0.2 &2& B1.5 & $-$7.29$\pm$0.46 & 199$\pm$7 & 229$\pm$5 \\
 & 68 & 0.5 &2& B9 & $-$6.84$\pm$0.23 & 353$\pm$7 & 99$\pm$5 \\
 Be 86 & 9 & 0.25 &6& B2.5 & $-$4.83$\pm$0.14 & 367$\pm$1 & 383$\pm$3 \\
 & 26 & 0.5 &6& B4 & $-$19.02$\pm$1.1 & 151$\pm$6 & 491$\pm$5 \\
\hline
\end{tabular}
\end{table}

The estimated rotational velocity of the star, as well as the disk is
basically the Vsin{\it i}, which is the projected component.
In general, we expect the disk to trail behind the star,
but we can see that in certain cases the rotational velocity of the disk
is higher than that of the star.
The stars 181 (NGC 6910), 9 (Be 87) and 68 (Be 87) have disk
velocity higher than the star. All the three stars have either
double-peaked H$_\alpha$ or asymmetric profile.
In principle, one has to de-convolve the peaks and then estimate the individual FWHM.
Since the spectral resolution is poor, we are unable to deconvolve the profile. Thus,
we have over estimated the disk velocity. Thus, excluding these three cases, the
rest of the stars show faster rotation, when compared to the disk.

It will be interesting
to study the relative rotational velocity between the disk and the star. Since the
projection angle will contribute identically to both the velocities, the relative
velocity is assumed to be independent of the projection angle {\it i}.
This relative velocity could
be a function of spectral type and hence we consider 5 stars which are of
similar spectral type. The stars considered are
the emission stars Be 87(38), NGC 6910 (26), Be 87(15),
IC 4996(23) and Be 86(9). We have estimated
the difference in rotation velocity between the star and the disk and
it is plotted against the rotation velocity of the star (figure 19).
The stellar rotational velocity
is found to be between 200 -- 400 kms$^{-1}$. The two stars in Be 86 have
relatively large velocities (one is of later spectral type).
The disk is found to lag behind the
star by 0 - 40 kms$^{-1}$ for four stars, For one star, the disk is slower by
68 kms$^{-1}$. This star happens to have the highest value of equivalent width for H$_\alpha$,
which indicates a heavier disk.

We find that out of the 9 emission stars, most are likely to be CBe stars.
There may only be at the most one-two HBe candidates, if at all.
Also, the rotational velocity of the emission stars are in the range of those of
the CBe stars, supporting their CBe nature.
We see that the CBe phenomenon starts very early
in the evolution of these stars, by about 2 -- 7 Myr. Since these stars
are well below the turn-off
of the cluster, the CBe phenomenon starts much before the star evolves from the MS.

Capilla et al. (2000) found that younger clusters (age $\le$ 10 Myr) do not contain Be stars.
Clusters in the age interval 10-30 Myr are rich in Be stars. Almost all of them are
of spectral types earlier than B5, while late-type Be stars are scarce. These results
point towards an evolutionary interpretation of Be phenomenon, in the sense that Be stars
are close to the end of their MS life time. Capilla et al. (2000)
did not find any Be stars in NGC 6910.
The clusters studied here all have a turn-off age less than 10 Myrs and they are found
to have 9 emission stars which are likely to be CBe candidates. 2 stars are of
spectral type B5 and one of B7, which indicates the possibility of late type Be stars
present in young clusters which in turn means that the CBe phenomenon need not be an
evolutionary effect. Fabregat (2007) suggested that CBe phenomenon is an evolutionary effect
appearing at the second half of the life in the MS of a B star.
But this study suggests that CBe phenomenon can happen during the core burning
initial phase in the MS life time of the star.
\begin{table}
\caption{The estimated duration of star formation in the five clusters.}
\vspace{0.5cm}
\centering
\begin{tabular}{cccc}
\hline
Cluster & Turn-on & Turn-off & Duration of \\
        & age (Myr) & age (Myr) &  star formation (Myr) \\
\hline
 IC 4996 & 0.5 & 7.5$\pm$3 & 7(continuous) \\
 NGC 6910 & 0.5 & 6.5$\pm$3 & 7(continuous) \\
 Berkeley 87 & 0.2 & $\sim$2 & 2 (continuous) \\
 Biurakan 2 & 0.5 & $\sim$6 & 5 (continuous/recurrent)\\
 Berkeley 86 & 0.2 & $\sim$6 & 6(continuous/recurrent)  \\

\hline

\end{tabular}
\end{table}
\section{Location of clusters and direction of star
 formation in the Cygnus Region}

In the Cygnus OB region, 5 clusters are
studied. The estimation of the turn-off age and turn-on
 age of the clusters along with their distance provides a
reasonable interpretation about the direction of
propagation of star formation in the Cygnus OB
star forming complex.
     The longitude and distance to the cluster is used to derive
their location in the Cartesian Coordinate system as shown in Figure 20.
The estimated duration of star formation in the clusters studied are tabulated in table 5.
The location of clusters along with their age is used to understand
 the star formation.
This region, located between the galactic longitudes $l = 70^o - 80^o $,
has eight more open clusters, for which reliable distance and age estimates are available.
We include these clusters also, as shown in figure 21, to understand the star formation.
The clusters included are Collinder 419, Collinder 421, Ruprecht 172, NGC 6913,
NGC 6871,  Biurakan 1 and ASCC 111. The first four clusters are
located closer to us, closer than 1200 pc and the rest of the three clusters are
located very close to Be 86, Be 87 and Biurakan 2 . The ages as given in WEBDA for these
three clusters are 9 Myr, 18 Myr and 11 Myr, respectively.

We interpret this figure keeping in mind that there may be significant error
associated with the estimated distance. The clusters can be grouped into
three groups, the first one is located
around 1 kpc, the second group is located at $\sim$ 1500 pc and the third group, beyond
2000 pc. The farthest group consists of two clusters, NGC 6910 and IC 4996.
Both the clusters seem to have similar star formation history.
The second group seems to indicate a vigorous star formation, where the relatively
older clusters, Biurakan 2,
NGC 6871, Biurakan 1 and ASCC 111
could have formed first, then Berkeley 86 and very recently, Berkeley 87.
In both the groups, the duration of star formation is about 5 -- 7 Myr. We estimate
a short duration for the star formation, 2 Myr, in the case of Berkeley 87. The three clusters
studied here indicate an enhanced star formation in the last 1 -- 2 Myr.
Also, the major star
forming region with 6 clusters is located at $\sim$ 1500 pc, and this could be considered as
the most active star forming region within the longitude range $l = 70^o - 80^o$ and located at
$\sim$ 1500 pc. No preferential location for the young pre-MS stars were found in the clusters.
The emission line stars were found in 4 clusters and one was found to be devoid of such stars.
Therefore, all clusters in a star forming complex may not harbour emission line stars.
Thus, the recent star formation observed in the
Cygnus was started about 2 -- 7 Myr ago, depending on the location. This implies that
the star formation in large complexes can last up to 7 Myr.

\section{Conclusion}
The main conclusions of the present study can be summarised as follows:
\begin{description}
\item In the Cygnus region, 93 candidate pre-MS stars
and 9 stars with H$_\alpha$ emission spectra are identified in 5 clusters.
\item The duration of star formation (estimated as the difference between the turn-off and
turn-on age) is estimated for five clusters. This indicates that the star formation
in the clusters were going on for 2 -- 7 Myr. The recent star formation in the Cygnus
region started $\sim$ 7 Myr ago.
\item CBe phenomenon
can be found in very young MS stars which are just a few ( 2 -- 7) Myrs old.
This indicates that the CBe phenomenon need not be an evolutionary effect.

\section*{Acknowledgements}
This research has made use of the WEBDA database, operated at the Institute for
Astronomy of the University of Vienna. This publication makes use of data products
from the Two Micron All Sky Survey.
Bhavya B., would like to thank Indian Institute
of Astrophysics for supporting her for MSc. project and for her ongoing thesis project.

\end{description}

redpajama_set_name: RedPajamaArXiv


Check out this series of beautiful cards visualising what makes us who we are. Love. Creativity. Enjoyment. Curiosity. Friendship. Spirituality. Psychological research shows that we are all driven by the same things – but differ in how we prioritise them. 58 values guide every aspect of our lives, shaping who we are both personally and as a society.
This research inspired designer Genis Carreras – creator of Philographics – to produce The Values Deck: an accessible, user-friendly set of cards that make visible these invisible drivers of human behaviour.
6 fascinating Fact Cards, offering information on the different sets of values and how they influence our lives.
Fund it on Kickstarter until 12 March 2015!


text:
Jim le harponneur () est un film américain réalisé par Millard Webb et sorti en 1926.

Cette production de Warner Bros. a connu un grand succès aux États-Unis, et a eu un rôle culturel important en France.

Synopsis

L'histoire est très librement adaptée du célèbre roman d'Herman Melville, Moby Dick, et modifie en particulier la fin tragique en happy end. Jim, un des meilleurs harponneur d'Amérique est fiancé, mais son frère, jaloux, le fait tomber à la mer pendant une chasse à la baleine. Il se casse une jambe et doit être amputé.

Fiche technique
 Titre original:
 Réalisation : Millard Webb
 Scénario : Bess Meredyth, Rupert Hughes, Jack Wagner d'après Moby Dick d'Herman Melville
 Production : Warner Bros.
 Lieux de tournage :  San Pedro, Los Angeles
 Photographie : Byron Haskin, Frank Kesson
 Montage : Rupert Hughes
 Durée : 136 minutes
 Dates de sortie:
  ()

Distribution

John Barrymore : Captaine Ahab Ceeley
Dolores Costello : Esther Harper
George O'Hara : Derek Ceeley
Mike Donlin : Flask
Sam Baker : Queequeg
Sōjin Kamiyama : Fedallah
George Berrell : Perth
Sam Allen : Capitaine
Mathilde Comont : Mula
James O. Barrows : Rev. Harper
Vadim Uraneff : Pip
Frank Hagney : Daggoo

Critique
Ce film a contribué à l'évolution de la critique cinématographique en France: le , Léon Moussinac, critique au journal L'Humanité, publie une critique très négative de Jim le harponneur, titre français du film américain The Sea Beast. Deux semaines plus tard, Jean Sapène, directeur du Matin et propriétaire de la Société des Cinéromans qui distribue le film en France, intente un procès à Léon Moussinac, et publie un article dont le titre est « La Société des Cinéromans poursuit L'Humanité... pour crime de "critique" ! ». Lors d'un premier procès en , L'Humanité et Moussinac  sont condamnés à 500 F de dommages-intérêts, mais sont finalement relaxés en , ce qui crée la première jurisprudence en matière de critique de cinéma.

Notes et références

Liens externes

 Jim le harponneur, Fondation Jérôme Seydoux

Film américain sorti en 1926
Film d'action américain
Film d'aventure américain
Film fantastique américain
Film romantique américain
Film américain en noir et blanc
Adaptation d'un roman américain au cinéma
Film muet américain
Film de Warner Bros

redpajama_set_name: RedPajamaWikipedia


text:
Policy & Data Brief June 06, 2019
Are State Unemployment Systems Still Able to Counter Recessions?
by Michele Evermore
Areas of expertise: Retirement Security, Social Security, Unemployment Insurance, Worker Training Read Profile
Every Thursday, the U.S. Labor Department releases data on initial claims for unemployment insurance (UI). In tandem with the overall unemployment figures published the first Friday of every month, these data have long been considered key indicators of the nation's economic health.
Recent research, however, has identified a disturbing trend: workers are both applying for and receiving UI benefits at much lower rates than they have in the past, even compared to comparable points in previous economic cycles.
To the extent that these lower rates are the product of legislative and administrative hurdles—policies intended to discourage application for and receipt of benefits—it is time to consider whether states are prepared to withstand future recessions.
The share of eligible jobless workers who actually apply for and receive unemployment insurance—referred to as the "take up" rate—is important in three ways. First, and most obviously, it is important that people have access to needed benefits so that they can make ends meet when they find themselves involuntarily unemployed. Second, these benefits are important to the broader economy, serving both as stabilizer and stimulus when there is a financial downturn. Finally, a stable take-up rate is important for understanding and interpreting economic trends. When policy decisions drive the take-up rate downward, it can rob analysts of an important tool in understanding the economy.
This paper seeks to examine the declining take-up-rate trend; the intersection of take-up rates and recipiency; and the need for policy changes that would increase UI take-up and recipiency for workers who have earned these benefits. These are necessary in order to maintain the reliability of UI as a counter-recessionary tool and also the validity of initial claims data as an economic indicator.
Understanding Recipiency and Replacement Rates
An important metric that intersects with take-up is the recipiency rate—the overall percentage of jobless workers who are receiving UI benefits. Workers may take-up benefits but lose them later because of continuing eligibility requirements, affecting overall recipiency. Another important metric to understand is the replacement rate—that is, how much income unemployment insurance replaces.
In December 2017, we published Closing Doors on the Unemployed, an extensive examination of the dramatic decline in UI recipiency since the Great Recession. We found that states, faced with the challenge of replenishing diminished UI trust funds, chose cutting benefits over replenishing those funds as the means to restore solvency. This approach ignores the reality that entering a recession with an underfunded UI trust fund is a highly unwise and substantial risk for any state; cutting benefits to get to solvency is certainly the wrong avenue to take when preparing for a recession.
Entering a recession with recipiency and replacement rates that are too low to provide economic stimulus is also a significant risk. A major policy goal of the UI system is to maintain economic activity levels during downturns by giving involuntarily unemployed workers enough spending power to keep their families and communities afloat. Reducing both the recipiency and the purchasing power of these benefits discourages people from applying at all, and these factors combined erode more than the quality of individual lives; it is dangerous for the entire community.
Download Complete Publication
[1] Many states have adopted alternative base periods to establish eligibility for workers who do not meet eligibility under the normal base period.
[2] Wayne Vroman, Unemployment insurance recipients and nonrecipients in the CPS, in Monthly Labor Review (Washington, DC.: Bureau of Labor Statistics,, 2009)
[3] Alix Gould-Werth and H. Luke Shaefer, Unemployment Insurance participation by education and by race and ethnicity, in Monthly Labor Review (Washington, D.C.: Bureau of Labor Statistics, 2012)
[4] United States Government Accountability Office, UNEMPLOYMENT INSURANCE: Low-Wage and Part- Time Workers Continue to Experience Low Rates of Receipt, (Washington, D.C.: Government Accountability Office, 2007)
[5] Stephane Auray, David L. Fuller, and Nicolas Lepage-Saucier, Why Do Half of Unemployment Benefits Go Unclaimed?, (2018)
[6] https://oui.doleta.gov/unemploy/bqc.asp Table IPIA 2017 Improper Denials by Cause
[7] https://oui.doleta.gov/unemploy/bam/2007/bam-cy2007.pdf pp. 15-17
[8] Vroman, Unemployment insurance recipients and nonrecipients in the CPS
[9] Gould-Werth and Schaefer, Unemployment Insurance participation by education and by race and ethnicity, p. 32
[10] Auray, Fuller, and Lepage-Saucier, Why Do Half of Unemployment Benefits Go Unclaimed?
[11] Auray, Fuller, and Lepage-Saucier, Why Do Half of Unemployment Benefits Go Unclaimed?, p. 2
[12] United States Government Accountability Office, UNEMPLOYMENT INSURANCE: Low-Wage and Part- Time Workers Continue to Experience Low Rates of Receipt
[14] Dante Deantonio, Why Are Unemployment Insurance Claims So Low?, (New York: Moody's Analytics, 2018)
[15] George Wentworth, Closing Doors on the Unemployed, (New York: National Employment Law Project, 2017)
[16] Gary Burtless, When the next recession hits, will unemployment benefits be generous enough?, (Washington, D.C. Brookings Institution, 2018)
Closing Doors on the Unemployed: Why Most Jobless Workers Are Not Receiving Unemployment Insurance and What States Can Do About It
Fact Sheet, FAQ
Closing Doors on the Unemployed—Improving UI at a Glance
A Plan to Improve Unemployment Protections in America
Unemployment Insurance Policy Advocate's Toolkit

redpajama_set_name: RedPajamaCommonCrawl


text:
Our Ales
The Dragons
Stuart Deeley - Dragon Lord (Head Brewer)
The 'Walter White' of the brewing world; a Chemical Engineer by trade Stuart spent over 30 years working in chemical and food manufacturing industries. He finally retired in 2013 to pursue his dream of creating the best beers in the world.
Alex Moore (Will) - Experimental Alchemist
Alex has been involved in with the pub trade for most of his adult life. He's also worked in it.
As part of Spirit Amber group he has worked in pubs across the North West and North East of England and knows a fair amount about the varying tastes across regions and even between pubs.
Driven by a passionate desire to brew his own recipes, Alex is incredibly enthusiastic when faced with bags of hops and other ingredients and gained the nom-de-brew of Experimental Alchemist after somebody left their cat nearby whilst he was brewing. Unfortunately we are now out of 'mittens ale' as the Dragons took quite a liking to it.
Matt Deeley - Apprentice Magician
Drawn to the company by the combined need for beer and money, Matt is the computer Brains behind the team.
The Dragons have given up trying to eat him despite the fact he holds no direct benefit for them (he very rarely actually makes the beer). This is mainly because, despite their best efforts, they can't help but succumb to instant onset narcolepsy every time they get near to him. Usually because he's waffling on about quad cores and hyper threaded doo dahs and gigabytes of RAM and offline backups and server... zzzzzzzzzzzz....
He has been seen to draw beer at events; occasionally selling it as well. His current pride and joy is an angram system set up in the utility room - creating a triangular route between lounge, loo and beer tap. Most recently he has installed himself as a permanent fixture at the Sandstone Inn, our public house, as resident Landlord. This has, of course meant he has even greater access to intoxicating fluids and now has very little idea what century we are in.
There is conjecture that Lazy Dragon is his favourite beer for the obvious reason - a rumour the he has strongly denied (he was drinking a pint of it at the time).
He has been given the title as apprentice magician because quite frankly no one is entirely sure how he does what he does. He clicks a few buttons, mumbles a few words (which won't be repeated here for fear of further attacks of narcolepsy) and out comes something that, well, frankly no one understands anyway, but it looks pretty. Sounds like Magic to us!


At least 7 years' experience on primarily economic development / governance development projects.
At least 5 years of this working in a role that included national / state government policy and reform, business regulatory reform and investment climate issues.
Demonstrated track record of a lead role in facilitating successful reform (through to practical implementation) in at least two of the thematic areas mentioned above.
Experience in business environment analytics and strategy.
At least 8 years' experience in business in an investment/consultancy role advising primarily private sector clients or working within a multinational business.
Advice to multinational enterprises on location and set up in new countries including around issues of land, tax, customs, workers' rights and other regulation.


Swimming pools are popular in the United States. In fact, they are so popular that you may even have one in your own backyard. If you do, which type of swimming pool do you have? Do you have an in-ground pool or an aboveground pool? If you answered aboveground, how do you get in and out of your pool? If you are like most other pool owners, you climb in and out by using a ladder. How would you feel if there was an easier way to enter and exit your pool? When it comes to aboveground pools, there are many pool owners who wish that they were more attractive. While most aboveground pools come with modern décor, many are still unflattering. This is often due their large bulky size and unflattering pool ladders.
If you are interested in improving the appearance of your aboveground pool, you may want to examine what a pool deck can do for you. Pool decks are similar to traditional decks, the ones that attach to most homes. Most of these decks are made of wood. What is nice about pool decks is that they can stand alone or they can be attached to another fixture, such as a home. Pool decks can also come in a wide variety of different sizes.
Many pool owners have pool decks that circle around their entire pool, while others only have a few feet of deck space. If you are interesting in attaching a pool deck to your aboveground pool, you can choose to have a large or small deck, the decision is completely yours. If you are interested in having a pool deck added on to your pool, you will have a number of different options, when it comes to purchasing one. If you are looking for a pool deck that is small in size, you may be able to order a pre-made one. Similar to pre-made pool houses, pre-made pool decks are constructed by trained professionals and then transported to your home for installation. While it is nice to have a pre-made deck installed, you may find that their cost is high, when compared to your alternatives. If you are looking for a cheaper alternative, you may want to consider constructing your own pool deck. With the proper supplies, which can be obtained from most lumber yards, you should easily be able to make your own pool deck. If you are inexperienced in construction, you may be able to find a number of free instruction guides online. These instruction guides may provide you with detailed directions and helpful tips for making your own pool deck.
However, even with a detailed instruction booklet or manual, you may be unable to build your own deck. If this is the case, you may want to seek professional assistance. When it comes to seeking professional assistance, with the construction of a pool deck, you will want to seek help form a local contractor. If you are unfamiliar with any contractors in the area, you can easily find a few of them by using your local phone book or the internet. To find the best prices, you will want to contact a number of different contractors and request free quotes. This is important because not all contractors charge the same amount of money. By going with the first contractor you meet, instead of comparing fees, you may end up paying too much money for your new pool deck. By keeping the above mentioned points in mind, you may be able to find a pre-made pool deck or have one constructed for a reasonable price. As previously mentioned pool decks help to increase the appearance of most aboveground pools. In addition to increasing the appearance, you may also find that they make it fun and easy to enter or exit your pool.
PPPPP Word Count 640 .


Investors Alert !! 12.84 acres with all mineral rights and royalties plus 3 story house with great potential for country living ! Kitchen, dining room, bath & bedroom on main floor and 2nd floor so could easily be rental. Multiple barns for storage, work shop or animals lots of possibilities ! Beautiful pond behind barns. Lots of road frontage ! Being sold ''as is''.


/Trading /Where can I find more details on FoxTrader?
We have partnered with Reliable Software Pvt. Ltd. to offer you a new revolutionary trading experience with sophisticated charting experience.
FoxTrader bridges the gaps in your trading experience by providing data analysis, back testing and trading under one roof.
As a promotional offer, you get 15 days Free Trial to use FoxTrader. Click here to know more on charges.
You can install FoxTrader by downloading FoxTrader setup. Follow through the self-explanatory installation steps. Fill up your details, select the active segments and login with your Trade Smart Online Credentials. You can explore it to the extent you like it to.
You can visit the youtube channel for various videos on features that are integrated in FoxTrader.
Get support on anything related to FoxTrader @ 022 – 62858700 / 40918900. You can alternatively send email to support@reliable.co.in for any issues or technical strategy construction.


What started as a father-son putt-putt outing has turned into a full-fledged adventure of disc golf where nearly every inch of grass at Butler Elementary is taken up by a father, a son or a flying Frisbee. The annual Butler Father & Son Disc Golf Classic has been around for 25 years, and judging from the number of fathers and sons who participate, it still has fairly strong legs.
Fathers and sons break up into teams and play 12 holes of disc golf, covering pretty much every area of outdoor school grounds. The object of the game is to complete each hole in the fewest number of throws, starting from a tee area and finishing at the disc pole hole. Just like golf, teams with the lowest total cumulative score win.
A few years ago, Butler's Dad's Club purchased a number of these disc pole holes, which are poles that extend up from the ground with chains and a basket where the disc lands. Shifting from putt-putt golf turned out to be a good idea, Butler Dad's Club President Jose Amate said.
Butler administrators love it, particularly the physical education teachers, who say disc golf is a good fitness sport and one that is accessible to all ages and fitness levels. You don't have to be athletically gifted to throw a Frisbee.
Butler's Father & Son Disc Golf Classic is just one of the major events organized and hosted by the Dad's Club. The big Daddy-Daughter Dance is another.
Former club president Dieter Scholtlyssek is a Butler dad who has been around for years and still has one daughter left at Butler.
Pictured: Sixth grader Hagan T. takes the competition seriously at Butler Elementary's annual Father & Son Disc Golf Classic.


"Awesome show , band just gets tighter as time goes.Really no one to compare them to anymore,just them as them. It's as if they have found their own way now. The Voodoo is the best place to see them live. Frat boys in polo shirts that are trying to show off for their boy friends, who don't know a Crowes song from Coldplay should stay at home with their mom. Anyway, one of the best shows in years .PEACE"


Stevia, Stevia rebaudiana, is a food flavouring. The leaves are used in South America to sweeten their Mate drinks. Leaves are 300 times sweeter than sugar but with no calories. Fresh or dried the leaves are used to flavour and sweeten drinks, baked foods, preserves and diet food. A treatment for hypoglycaemia and a digestive aid. Stevia is native to mountainous areas of Southern Brazil and Paraguay. Prefers rich, moist well drained soil in a protected sunny position. Clusters of tiny white flowers in summer. Frost and drought tender. Perennial deciduous plant; may die-back to ground level. Grows to 1m x 0.6m.
Be the first to review "Stevia, seed" Click here to cancel reply.


text:
package web.domain;

import org.springframework.security.oauth2.common.OAuth2RefreshToken;
import org.springframework.security.oauth2.provider.OAuth2Authentication;

/**
 * Token which holds data regarding the OAuth2 Authentication Refresh token.
 *
 * Based on the work of: https://github.com/iainporter/oauth2-provider/
 */
public class OAuth2AuthenticationRefreshToken {

    /** The ID of the token. */
    private final String tokenId;

    /** Reference to the refresh token. */
    private final OAuth2RefreshToken oAuth2RefreshToken;

    /** Reference to the authentication object. */
    private final OAuth2Authentication authentication;

    /**
     * Constructor to create a new refresh token.
     *
     * @param oAuth2RefreshToken - The OAuth2 Refresh token.
     * @param authentication - The Spring Security Authentication object.
     */
    public OAuth2AuthenticationRefreshToken(OAuth2RefreshToken oAuth2RefreshToken, OAuth2Authentication authentication) {
        this.oAuth2RefreshToken = oAuth2RefreshToken;
        this.authentication = authentication;
        this.tokenId = oAuth2RefreshToken.getValue();
    }

    /**
     * Returns the ID of the token.
     *
     * @return String - Token ID
     */
    public String getTokenId() {
        return tokenId;
    }

    /**
     * Returns the OAuth2 Refresh token.
     *
     * @return OAuth2RefreshToken - Refresh token
     */
    public OAuth2RefreshToken getoAuth2RefreshToken() {
        return oAuth2RefreshToken;
    }

    /**
     * Returns the OAuth Authentication object.
     *
     * @return OAuth2Authentication - Authentication object.
     */
    public OAuth2Authentication getAuthentication() {
        return authentication;
    }
}

redpajama_set_name: RedPajamaGithub


text:
https://www.wsj.com/articles/venezuela-opposition-threatened-by-embezzlement-allegations-11560904989
Venezuela Opposition Threatened by Embezzlement Allegations
Leader Juan Guaidó's team requests Colombian prosecutors investigate two opposition activists
Mr. Guaidó's movement has lost momentum against Mr. Maduro after a five-month pressure campaign of street demonstrations and international sanctions that have failed to unseat the authoritarian leader.
Photo: rayner peña/epa/Shutterstock
Kejal Vyas
@kejalvyas
kejal.vyas@wsj.com
Juan Forero
@WSJForero
juan.forero@wsj.com
BOGOTÁ, Colombia—Venezuela's political opposition welcomed funds from private donors and foreign governments as the movement to remove authoritarian leader Nicolás Maduro gained momentum earlier this year, with money earmarked to help hundreds of Venezuelan soldiers who defected to neighboring Colombia.
But now, accusations that two opposition activists pilfered tens of thousands of dollars from those funds are threatening to become an embarrassment for a coalition that is heavily dependent on the largess of dozens of countries, including the U.S., which is allied with its chief, Juan Guaidó.
On Tuesday, Mr. Guaidó's aides in Bogotá, scrambling to contain political fallout that could curtail foreign aid in the future, requested that Colombian prosecutors investigate how the two activists allegedly embezzled as much as $60,000.
The money, from private donations, had been allotted to pay some of the costs of hotel rooms, meals and transportation incurred by Venezuelan military deserters, whom Mr. Guaidó had heralded as heroes after they broke from Mr. Maduro and crossed the border to Colombia.
The two accused activists, Rossana Barrera and Kevin Rojas, had been appointed to manage some $100,000. They haven't been charged and couldn't be reached for comment.
How 7.4 Tons of Venezuela's Gold Landed in Africa—and Vanished (June 18)
Venezuelans' Latest Woe: Gas Lines That Last for Days on End (June 10)
In a Blow to Maduro, Russia Withdraws Key Defense Support to Venezuela (June 2)
Venezuela Negotiators Agree to New Round of Talks (May 25)
Maduro Moves to Reassert Authority, Arrest Opposition Leaders (May 2)
Venezuela Crisis: Violence Erupts as Guaidó Calls for Uprising (May 1)
Humberto Calderón Berti, Mr. Guaidó's representative in Bogotá, said he requested the Colombians investigate because the opposition wants to differentiate itself from Mr. Maduro's regime, which is accused of rampant graft. The watchdog organization Transparency International says Venezuela is perceived as one of the most corrupt in the world, ranking 168 of 180 countries.
"Our message to the country is that we're different, we are going to act with absolute transparency," Mr. Calderón said in a press conference Tuesday at the attorney general's office here after meeting Colombia's top prosecutor, Fabio Espitia Garzón.
The allegations, made public earlier by the PanAm Post, an anti-Maduro news site, come as Mr. Guaidó's movement has lost momentum against Mr. Maduro after a five-month pressure campaign of street demonstrations and international sanctions that have failed to unseat him.
A recent poll by Venezuelan pollster DatinCorp found that about 36% of respondents recognized the young opposition leader as Venezuela's legitimate president, down from 49% in February. Mr. Maduro was seen as president by 41%, up from 34% of respondents, though Venezuelans blame him for the economic mismanagement that has caused hyperinflation, food shortages and the exodus of millions of migrants.
Humberto Calderon Berti, opposition leader Juan Guaidó's representative in Bogotá, said he requested the Colombians investigate the allegations because the opposition wants to differentiate itself from Nicolás Maduro's regime.
Photo: Leonardo Munoz/EFE/Zuma Press
Mr. Guaidó is facing increased pressure from factions within his own opposition coalition who reject recent negotiations brokered by Norway and advocate foreign intervention to remove Mr. Maduro.
"In reality, there's only one real option on the table. That option is force," one opposition leader pushing for the hard-line approach, María Corina Machado, said in a June 12 public letter to Mr. Guaidó.
At the same time, high-ranking officials in the Maduro government, most of whom face U.S. sanctions for alleged corruption and rights abuses, were quick to take advantage of the allegations against their rivals.
Mr. Maduro's attorney general in Venezuela, Tarek William Saab, said that "villas and castles" were promised to deserting Venezuelan military officers "but they were left in the street."
He blamed Mr. Guaidó, whom the regime considers a traitor, for the alleged embezzlement. "He should be ashamed, making declarations when he's head of a corruption Mafia," he said.
Legal advisers working with Mr. Calderón said they found evidence that the accused activists filed overpriced and fictitious hotel invoices. Mr. Guaidó's administration has been the beneficiary of more than $90 million in humanitarian aid from the governments of Canada, the U.S., the U.K. and Germany. The funds, Mr. Guaidó said, are largely managed by the donors and not by the group of Maduro opponents he heads. He noted that the money for the soldiers was separate from humanitarian donations from foreign governments.
"We're not going to let this hurt and smear all of the effort that we've made" on humanitarian aid matters, said Lester Toledo, a Venezuelan lawmaker in exile who is working with Mr. Guaidó's team. "The first thing that we should be asking for is prison for the corrupt ones."
Colombia's attorney general's office said it would begin an inquiry that could lead to a formal investigation.
For Mr. Calderón, what to do with military defectors has become a serious dilemma when Colombia has already received 1.3 million Venezuelans fleeing their country.
Many of the soldiers had crossed into Colombia heeding Mr. Guaidó's ill-fated call on Feb. 23 to foment a military rebellion. They later grew disgruntled after Colombian officials and people in Mr. Guaidó's camp told them they would not be converted into a mercenary force. In recent weeks, the Colombian government stopped paying their hotel bills, instead offering monthly stipends and work permits so they could settle into civilian life.
Mr. Calderón said Colombian intelligence authorities told him two months ago to look into alleged misappropriation of money earmarked for the deserters.
"Unfortunately, in our country, we have grown accustomed after 20 years of a dictatorial regime to brush off these acts," Mr. Calderón told reporters.
With hunger spreading, Venezuelans have an increased intolerance for graft and a serious investigation could help draw a distinction between Mr. Guaidó's movement and Mr. Maduro's government, said Moisés Naím, a Venezuelan author and former trade minister. The regime in Caracas is blamed for squandering hundreds of billions of dollars of oil revenue through graft, bankrupting what was once Latin America's wealthiest nation, economists say.
Mr. Maduro's government has said such claims are designed to debilitate his government.
"This can be a golden opportunity for Guaidó," Mr. Naím said.
Write to Kejal Vyas at kejal.vyas@wsj.com and Juan Forero at Juan.Forero@wsj.com
Appeared in the June 19, 2019, print edition as 'Embezzlement Allegations Hit Venezuelan Opposition.'


text:
Anurodh (1977) | Rajesh Khanna, Ashok Kumar, Vinod Mehra, Asrani, Simple Kapadia, Nirupa Roy, Utpal Dutt, Dina Pathak, R
Anurodh (1977) | Hindi Movie | 6.9/10 | Synopsis : Mr. Choudhary does not approve of his son, Arun, indulging in singing
Anurodh
SYNOPSIS : Mr. Choudhary does not approve of his son, Arun, indulging in singing songs and music. He wants him to be a businessman like himself. Out of fear of his father finding out about his ...
STAR CAST : Rajesh Khanna, Ashok Kumar, Vinod Mehra, Asrani, Simple Kapadia, Nirupa Roy, Utpal Dutt, Dina Pathak, Rita Bhaduri, Abhi Bhattacharya, Preeti Ganguli, Asit Kumar Sen, Birbal, Mrinal Mukherjee, Amar Nath
GENRE : Drama | Family
DIRECTOR : Shakti Samanta RATINGS : 6.9/10
India - Hindi Aatish
India - Hindi The Great Gambler
India - Hindi Hamare Tumhare
India - Hindi Dhongee
India - Hindi Do Ladke Dono Kadke
© 2018 Scratchu.com | Contact Us | Privacy | Terms ✉ Anurodh (1977) | Rajesh Khanna, Ashok Kumar, Vinod Mehra, Asrani, Simple Kapadia, Nirupa Roy, Utpal Dutt, Dina Pathak, Rita Bhaduri, Abhi Bhattacharya, Preeti Ganguli, Asit Kumar Sen, Birbal, Mrinal Mukherjee, Amar Nath - Anurodh (1977) | Hindi Movie | 6.9/10 | Synopsis : Mr. Choudhary does not approve of his son, Arun, indulging in singing songs and music. He wants him to be a businessman like himself. Out of fear of his father finding out about his ... ... Watch Online!!!


text:
Chip shortage to last well into 2022 Electronics360 Latest Industry News | by Deanna Parenti August 17,2021
Author: Peter Brown
The situation in the semiconductor supply chain is not improving quickly and now experts believe the chip shortage will last deep into 2022.
The constrained situation is likely to last until at least into the mid-point of 2022 and that is without surprises in the market such as the deep winter storm that impacted much of the Southwest last year. If COVID-19 continues to persist globally, this could be another wrinkle in extending the shortage further.
AUTOMOTIVE CHIP STRUGGLES CONTINUE
Initially, when the supply chain issues started, the automotive market was looking at constraints lasting the entirety of 2021. The automotive market was hit hard by the supply chain issues caused by COVID-19 and automotive OEMs were slower to secure capacity after the initial slowdown.
When suppliers saw demand return in the fourth quarter, which is generally not a huge production period for the automotive market, semiconductor manufacturers were already busy producing consumer electronics and other parts and no capacity was available.
Eight months later, the front-end has improved since the fire that destroyed a portion of the 300 mm line at Renesas' Naka and the ice storm that crippled the supply chain in Texas last year. However, the back-end is starting to bottleneck, according to Phil Amsrud, senior principal analyst for automotive at IHS Markit.
"Therefore, just adding fab capacity won't fix everything on its own," Amsrud said. "The back-end is limited because of lead frames, substrates and resins and a lot of the back-end facilities are in countries with low COVID vaccination rates. As the Delta variant spreads, it is impacting these facilities. For example, Malaysia shut down because of COVID."
With the Delta strain of COVID-19 running through many countries, it is still unclear how far it could impact the supply chain and if other areas will be forced to halt or suspend operations. If this happens, it could potentially push the chip shortage further into 2022.
LONGER ORDERS, HIGHER PRICES
One interesting trend is that automotive suppliers are accepting the new conditions of the chip shortage including longer firm orders and price increases.
"The suppliers who are complying with these conditions have a better chance of getting what they want than those who don't," Amsrud said. "Also paying expediting fees are another option to move to the head of the line, and all things being equal automotive may start out closer to the head of the line, but it's not the case that automotive gets everything that they want first and everyone else is fighting over what's left."
EQUIPMENT LEAD TIMES GROWING
One other problem that is emerging is the lead times for semiconductor equipment. Whether it is the back-end or front-end, semiconductor equipment is critical to expanding capacity.
Equipment lead times have increased because companies cannot get the semiconductors necessary to build them, leading to a catch-22 situation.
"The biggest challenge continues to be knowing the real demand," Amsrud said. "We call this the toilet paper effect because when COVID first hit the demand for toilet paper skyrocketed. A similar thing happened with semiconductor demand, so the supply chain continues to struggle to know how much to make of what specific devices. Even after additional capacity is online, knowing what to make is still key to helping everyone inside and outside of automotive get enough of what they need.
DISTRIBUTORS SEEING SIMILAR
Digi-Key, a leading electronics distributor, also sees the chip supply chain remaining tight through mid-2022.
"There are some areas of capacity coming online but much of that is not until the end of this year or next year early-mid 2022," said David Stein, VP of global supplier management at Digi-Key. "There are many different end markets that are causing this lead time for shortage of products. Today, as many as eight different verticals/end market segments are driving demand for the consumption of product."
The cycles of the semiconductor industry have changed in this regard where one or two end markets were driving the electronics market, Stein said. Now, when a market slows, there are others such as medical, automotive, 5G, industrial automation, internet of things, consumer or computer and more markets available to pick up the slack.
But this also means that demand for electronics is higher than ever before, meaning more capacity is needed from more companies. Until more capacity is available, the shortage will persist.
The demand for semiconductors is not expected to slow down either as growth of about 5% is expected over the next decade as these markets continue to want more chips.
Supplyframe, an e-commerce vendor that runs the electronic component sourcing site Findchips, sees the constraints in the supply chain pushing into the first quarter of 2023.
"One customer described the current environment as a 'game of whack-a-mole,' and we can see the ripple effect moving inconsistently over time and across adjacent sub-commodities," said Richard Barnett, CMO of Supplyframe. "Component suppliers and distributors know they have to reduce inefficiencies in their quoting process and work more directly with end customers to meet their needs."
To contact the author of this article, email PBrown@globalspec.com
Source: Chip shortage to last well into 2022 | Electronics360


text:
Q: Can't choose framework for segmentation_models library in python I am trying to build a ResNet34 model using segmentation_models(sm) library in python. The sm library uses keras framework by default when importing, but I am working with tf.keras to build my datasets used for training and testing.
The documentation says that in order to change the default framework I should either use an environmental variable SM_FRAMEWORK=tf.keras before importing (which I tried but it didn't work) or set it using the method set_framework (which doesn't show up in the suggestions/it says it doesn't exist when I try to execute it).
Is there any other way to overcome this problem?

A: I trained model on colab and I used :"%env SM_FRAMEWORK=tf.keras" to set the environment to tf.keras and it worked perfectly.

redpajama_set_name: RedPajamaStackExchange


text:
Founded in Newton, Massachusetts, in 1976, the Joanne Langione Dance Center was the first American youth dance school centered on a developmental and avocational model rather than a competitive one. Currently the dance center offers instruction to students between 9 months and 18 years old in classical ballet, modern dance, contemporary dance, jazz, hip-hop and tap dance, with ballet exams administered annually by the American Academy of Ballet. The school stages sixteen public performances each year.

The school's toddler dance program, "Playdance," developed upon the cognitive insight that the sequence of music and movement constitute "brilliant neurological exercises" in early childhood, was featured on the PBS Documentary and WCVB series for Lifetime, Your Baby and Child, with Dr. Penelope Leach. The school's first complement of "Playdance" graduates was featured on Bob McGrath's Sesame Street tour in 1988.

References

Further reading
Anderson, Leslie. "Boys wonder: "Shall we dance?" Boston Globe 14 March 1999: 1.
Carlock, Marty. "'Nutcracker' reaches into suburbs." Boston Globe 30 November 1997: 21.
Taylor, Denise. "A winding walk on New Year's Eve." Boston Globe 28 December 2006: 4.

External links
Joanne Langione Dance Center
Newton Patch entry

Private schools in Massachusetts
Dance schools in the United States
Educational institutions established in 1976
Schools in Middlesex County, Massachusetts
Newton, Massachusetts
1976 establishments in Massachusetts


Various law enforcement agencies were kept busy yesterday morning (September 10), serving a dozen search warrants between 6 a.m. and noon that resulted in 65 arrests and sizeable drug and weapons seizures.
The sweeps, dubbed "Operation Mountain Shadow," are the culmination of a yearlong drug investigation focusing on the communities of Poway and Ramona.
The total haul included 93 pounds of methamphetamine, 56 pounds of cocaine, 14 pounds of heroin, 5 pounds of prescription pills, and 30 grams (about one ounce) of marijuana. Authorities also confiscated $230,000 in cash, 76 firearms, and a live grenade.
All of those arrested face federal charges of conspiracy to distribute controlled substances, more charges are likely forthcoming. Depending on the severity of charges and arrestees' prior records, they face sentences ranging from probation to 25 years' imprisonment.
John Kitchin Sept. 11, 2013 @ 4:03 p.m.
A lot of the dope biz moved from El Cajon, Spring Valley, Santee, and Lakeside, up the road to more-rural Poway and even Ramona, where there are a lot fewer police. What fascinates me the most about the illegal drugs trade is the connections with both the Mafia and the Political Parties at the same time!


This 4 week, clinical rotation offers students the chance to learn how to provide quality healthcare to LGBTQ patients across medical specialties in an outpatient setting. Students will work with physicians and other providers in internal medicine, family medicine, infectious disease, endocrinology, pediatrics, adolescent medicine, OB/GYN, dermatology and psychiatry. A curriculum in line with current AAMC, proficiency-based standards will be presented and students will be given the opportunity to complete an advocacy or research project if desired. A clinical lead will serve to unify the experience and mentor the student towards a career working with LGBTQ patient populations.
The Oliver Goldsmith, MD Scholarship for the Promotion and Advancement of Culturally Responsive Care honors second- or third-year medical/osteopathic students who have demonstrated commitment to the advancement of culturally responsive care (CRC) through community service, clinical volunteering, or research. Each awardee will receive $5,000 toward his or her education, participate in a mentoring program with a KP clinician and complete a four-to-six week clinical rotation at a KP facility.


text:
Instructional Poi Videos
Zan Moore and Alien Jon's revolutionary Encyclo-poi-dia DVD's are now available for download. Right here.
The BEST Poi Instruction Available
Encyclopoidia Vol. 2 presents the theory, technique, and practice of poi with helpful visual simulations.
With 22 chapters, over 95 minutes of carefully crafted instruction, it covers all levels of spinning, from beginner to expert.
Isolations
Body Movement
And Tons More!
watch samples
By Donation!
Get the Encyclo-Poi-Dia
*The link above is for downloading Encyclo-Poi-Dia Volume 2.
The second volume is a much higher-quality resource, and it's recommended to start there.
If you want to continue your journey and dive into the archives, you can download Volume 1 here.
About the Encyclo-poi-dia
The Encyclo-Poi-dia was created by Zan Moore with the mission of offering high-quality learning resources in Poi spinning. His vision was to advance the art form in the long-term by training a new generation of flow artists with thoughtful, well-made content.
Zan learned to spin poi before YouTube existed, when spinners discussed new moves in text-based online forums. The release of "Encyclo-Poi-dia Volume 1" in 2006 was a landmark in the availability of instructional media for poi. Despite the video's 'homemade' quality and feel, this original DVD spread worldwide and taught over 6000 people how to spin poi.
Then, with the proliferation of free online videos, Zan was inspired to make a second video that would surpass the quality, organization, ease of use, and speed of learning available through free online content. The result was "Encyclo-Poi-dia Volume 2: A New System of Poi Spinning," released in 2009. For this video, Zan teamed up with Alien Jon to break down in detail a systematized approach to the types of possible motion and aesthetic interaction between poi and human bodies. This new version of Encyclo-Poi-dia included professional videography, 3-D computer modeling, and a plethora of professional poi artists giving performances and interviews about their craft.
Volume 2 finally achieved the vision of laying a foundation for the innovations and developments of a whole new generation of poi spinners.
After a few years, the DVD medium began to fall out of popular favor and the Encyclo-Poi-dia became relatively inaccessible until its release for digital download 2021. Willow and Zan, in offering this pay-what-you-can download of Encyclo-Poi-dia, wish to offer the educational material as a service to everyone with the desire to learn.
The DVDs originally sold for USD$25 (Vol 1) and USD$30 (Vol 2) each. Please, if you are able, offer some money as you download to help complete the circle of giving and receiving, and allow this service to remain free to all.
Thank you, and may your journey with poi be illuminating for your explorations of self, movement, and existing in the Universe.
Vol. 1&2 Comparison
© 2022 Willow Solow and Zan Moore