text:
\section{Introduction}

The search for extrasolar planets has been characterized recently
by a move toward the discovery of lower mass planets compared to the gas
giant planets of our Solar System.  While the techniques of
radial velocities, transits, and microlensing have already
proved to be successful in detecting extrasolar planets, the novel
idea of using transit timing variations (TTVs) to detect additional low-mass
companions in known transiting planetary systems \citep{ago05, hol05}
is a recent and exciting addition to the repertoire of planet detection
methods, which has not yet been widely applied.  The premise of the TTV method
is that a planet known to transit its host star will do so at a near-constant
period unless there is an additional planet in the system to perturb its
orbit.  In the case of a second planet in the system, the observer
will then view transits that deviate from a constant period on a level of
seconds to minutes, depending on the mass and orbital parameters of the
perturbing planet.   An analysis of transit timings in the TrES-1 system was
carried out by \citet{ste05} placing useful limits on the presence of
additional planets around that star.  They determine that a (2:1 resonant)
companion planet
in that system would generally need to have a mass comparable to or less than
an Earth mass.  A subsequent analysis performed on HST observations of HD
209458 by \citet{ago07} places similar limits on the presence of companion
planets in that system.  The addition of the {\it MOST} data now allows for
more stringent limits to be placed on such planets.

HD 209458 was the first star found to have a transiting planet
\citep{cha00, hen00} and remains the second brightest star known to have a
transiting planetary companion, making it suitable for a large number of
follow-up observations.  As more
transiting planets are discovered, it is becoming clear that HD 209458b
has an anomalously large radius for its mass when compared
with theoretical predictions \citep{lau05c}.  Speculation as to the
mechanism that is keeping the planet ``too large'' has led to several theories
including (i) additional sources of internal heating
such as strong winds \citep{gui02}, (ii) obliquity tides due to a disalignment
of the planetary spin axis and the orbit normal \citep{win05}, and
(iii) the presence of additional low-mass planets in the system inducing
eccentricity in the orbit of HD 209458b and causing ongoing tidal heating
\citep{bod01, bod03}.  The
first of these theories seems less likely, seeing as it would apply
to the radii of all of the transiting planets.  The latter two have remained
viable theories in explaining the anomalous radius of HD 209458b.

The TTV analysis that follows serves to shed some light on the presence of
additional planets in the system, and, together with previous observations,
now effectively rules out the third option listed above.  The Microvariability
and Oscillations of STars ({\it MOST}) satellite \citep{wal03, mat04} observed
HD 209458 in 2004 and 2005 as it passed through the satellite's Continuous
Viewing Zone (CVZ).  A combined total of 15 complete transits were
observed, with 12 of these being consecutive transits in 2005.  The combination
of the timings for these transits along with previously published transit
times by \citet{ago07} allow us to place strong limits on the presence of
additional planets in the system, which would be undetectable by other
currently available techniques.

\section{{\it MOST} Photometry}

Photometry of HD 209458 was obtained with {\it MOST} during 13.5 days in 2004
and 42.9 days in 2005.  {\it MOST} houses a 15-cm optical telescope feeding a
CCD photometer through a single custom broadband optical filter.  From its
820-km Sun-synchronous polar orbit, it can monitor stars passing through its
CVZ for up to two months without interruption.  {\it MOST} can collect
photometry in several
operating modes, including ``Direct Imaging'', in which a target star is
centred in a subraster on the {\it MOST} Science CCD for a combination of
aperture and PSF (Point Spread Function) photometry.

HD 209458 was observed in Direct Imaging mode, with exposures of 1.5 s
(as outlined in \citet{row06}).  The point-to-point precision for these
observations depends on the level of stray light scattered into the instrument
and can be as low as 3 mmag at times of very little stray light and as high as
20 mmag during instances of high stray light.  At low levels of stray light
this corresponds to a photometric error that is essentially equal to the
Poisson noise limit, whereas during times of increased scattered light this
can degrade to up to 1.5 times the Poisson limit (see Figure 2 in
\citet{row07}).  For the 2004 observations the sampling rate was varied to
obtain a higher
rate during phases of the known planet's secondary eclipse, resulting in an
average sampling of 5 individual exposures per minute.  For the 2005
photometry, the sampling rate
was 6 times per minute, a limit set by the data downlink capacity of the
{\it MOST} satellite in the Direct Imaging mode.

The reduction procedures for the 2004 photometry are described by \citet{row06}
and include corrections for stray light  due to Earthshine modulated with the
satellite orbit.  In the 2005 data, there was electronic
``crosstalk'' between the timing
of the Science CCD and the Attitude Control System (ACS) CCD onboard
electronics, with a timescale of about 3 days.  This manifested itself as a
subtle band of noise moving across the CCD subraster in about half a day.
Such
crosstalk added a non-Poisson component to the photometric noise, and
uncorrected could induce deviations of about 1 mmag on timescales of up to
a day.
By comparing the standard deviation of the background sky counts in the
subraster
against the square root of the mean sky count, we can trace the occurance of
crosstalk.  Corrections are then applied to the sky counts and the
instrumental magnitudes of HD 209458.  Other than this,
the 2004 and 2005 datasets have been uniformly reduced.

For this analysis, we have removed from the data set incidences of very high
levels of stray light (Earthshine) modulated at the satellite's orbital
period,
as well as times of passage through the South Atlantic Anomaly (SAA) when the
cosmic ray flux is high, and other instances of severe cosmic ray hits. This
reduces the total number of observations by about 12\%, but does not
seriously
reduce the coverage of the observations over the HD 209458b orbital period.
The reduced 2004 and 2005 light curves are shown in Figure~\ref{lightcurve}.

The pronounced gaps seen in Figure~\ref{lightcurve} in the 2004 data are
due to
onboard crashes caused by the testing of new software during those trial
observations.  The two shorter noticeable gaps in the 2005 light curve are
due
to especially severe SAA passages, which were removed from the data.  There is
some evolution of the level of scattered light during the 2005 data, dropping
slightly toward the end of the run, consistent with seasonal evolution
over six
weeks that has been observed for other targets.  There is also an unfortunate
coincidence for {\it MOST} observations of HD 209458, in that the giant planet
orbits at a period that is almost exactly 50 times the 101.413 min
orbital period of {\it MOST}.  Hence,
when we remove portions of the light curve with high stray light, these
consistently lie at the same phases in the light curve phased to the planet
transit period. We are alert to the possible effects on the transit timing
analysis, and have found that our results are not very sensitive to this
effect (see below).

\section{Transit Times for HD 209458b}

In computing our transit times we compare the {\it MOST} data against a model
transit curve, constructed using the formalism set forth in
\citet{man02} for a source with nonlinear limb darkening.  To determine the
orbital parameters for the model we start with those
laid out in \citet{knu07}, which in turn were determined by a multi-parameter
fit to data from the STIS
spectrometer aboard the Hubble Space Telescope (HST).  Noting that the
{\it MOST} transit light curve appears to be slightly deeper than this model
would predict, we then fit for the stellar and planetary radii by minimizing
the chi-square statistic for both variables on the composite phased and binned
{\it MOST} light curve.  Our values for the two radii differ somewhat
from the HST light curve but lie within the 1-$\sigma$ error
bars determined for that data set, with the {\it MOST} data implying a
planetary radius of 1.339 R$_J$ and a stellar radius of 1.118 R$_{\sun}$
(see discussion in \citet{row07}).  Nonlinear limb darkening parameters for
the {\it MOST} bandpass are derived from synthetic spectra calculated by R.
Kurucz
\footnote{See http://kurucz.harvard.edu/stars/hd209458}.  This is accomplished
by summing the spectra across the disk of the star then multiplying by the
throughput of the {\it MOST} optics and detector.
The resultant transit model has system
parameters that are given in Table~\ref{tbl1}, and this model is overlaid
on the phased and binned data in Figure~\ref{Model}.  We note that some
correlation in the residuals from this model (red noise) remains.   This is
most likely due to the stray light experienced by {\it MOST},
as it repeats at approximately the orbital period of the satellite, despite
reduction procedures to correct for this effect.  We pay particularly close
attention to the modulation of stray light to determine its effects on the
transit timing measurements as decribed below.

To determine times for each of the individual transits, the model light curve
is computed at impact parameters
corresponding with each of the {\it MOST} data points.  We then find the
center-of-transit time for each transit at which the $\chi^2$ value for the
fit to the data is minimized.  The resultant times
are presented in Table~\ref{tbl2} in HJD,
calculated using the IDL function helio\_jd \citep{lan93}.
We measured transit times for each of the 3 complete transits in the 2004
data and the 12 transits in 2005, then calculated the timing
difference from the expected times of transit, as shown in Figures~\ref{O-C}
and~\ref{O-C_2005}.  The expected times of transit are calculated by
adding the correct number of orbital periods of HD 209458b to the 2003
ephemeris from \citet{knu07}.  We note that our data agrees
with the orbital period and ephemeris of this previous work, since
our data points in Figures~\ref{O-C} and~\ref{O-C_2005} lie almost equally
above and below the line representing the expected times ($O - C = 0$).
As a reference, in Figure~\ref{O-C} we also show the times for the 4
transits observed in 2003 with STIS as reported by \citet{ago07}, who used a
similar method to determine transit times.

Our error bars are calculated using a bootstrapping Monte Carlo simulation
similar to the one described in \citet{ago07}.  For each transit we
shift the residuals from the best-fit transit model  (and their associated
errors) by a random number of points.  We then add the new residuals back
onto the transit model and recalculate the center-of-transit time using the
same procedure described above, thus maintaining the original point-to-point
correlations.  The goal realized by
this error analysis is to understand the effects of correlated noise in the
{\it MOST} light curve due to the repeating pattern of stray light.  The
resulting error bars in Figures~\ref{O-C} and~\ref{O-C_2005} are somewhat
larger than those obtained from a simple chi-squared analysis
(generally by less than a factor of 2, but occasionally by a factor of
several).  In addition, we have performed tests of
our sensitivity to the modulation of stray light during the {\it MOST}
satellite orbit by applying
more stringent removal of times of higher stray light.  This does not have a
significant effect on the transit times we determine and only reduces
unnecessarily the overall duty cycle of the observations.  It must also be
noted that, at the precision and time coverage of the {\it MOST}
data, intrinsic low-amplitude variations in the star HD 209458a may be present.
This may represent a fundamental limit in the systematic errors of the timing
data for this system.

Long-term and periodic trends in the data not associated with the HD 209458b
orbit could be a serious problem in limiting the accuracy of our transit times
so we have examined this issue closely.  This is especially true if a deviation
due to instrumental or satellite orbital effects was to occur during transit
ingress or egress.  As an example, consider a transit lightcurve in
which ingress has not been correctly normalized so that all of the points
are reported at a flux level that is slightly too low.  In this case, our
analysis method would report this transit as occurring earlier than it
actually did.  We have carefully identified
and corrected for possible long-term and periodic artifacts in the data to
produce a properly normalized light curve,
as described in \citet{row06}.  These include
(i) dips and rises in the lightcurve stemming from electronic crosstalk as
described in Section 2; (ii) cycle-per-day modulation of stray Earthshine due
to the Sun-synchronous orbit of {\it MOST}; and (iii) filtering of longer-term
trends in the data which might be instrumental, stellar or a combination of
both.

Another consideration in determining transit times is the importance of
having a light curve that
is well-sampled during ingress and egress, as this is where the timing
signal is most sensitive.  In the
case of a partial transit that is missing either ingress or egress, the
value adopted for orbital inclination (which determines the transit
duration) in the model light curve must be finely tuned to the true value.
Otherwise, the risk is that partially sampled transits could have large
systematic errors in their measured timings.  For the transit times
reported from the {\it MOST} data only complete transits were used.  In
particular, the second transit from the 2004 observations is not used in this
analysis since data are only available for half of it.  Note that the effect
of removing short intervals of very high stray light, (which often affects
ingress more than egress or vice versa) is negligible, since only a small
number of data points are actually removed from each transit.

\section{Limits on Other Close-in Planets in the HD 209458 System}

The two seasons of transit timing data from {\it MOST} allow us to look for
variations due to several effects: (1) orbital decay of planet HD 209458b
\citep{sas03}; (2) precession of its orbit \citep{mir02, lau05b, hey07};
(3) moons \citep{sar99, bro01};  and (4) orbit perturbations caused by
additional planets in the system \citep{ago05, hol05, ste06}.  The first two
effects would cause long-term variations in the observed time between
successive transits.  To check for these types of long-term drifts, our
best-fit times for the 15 observed transits from
{\it MOST} can be combined with the 13 transit times reported by \citet{ago07}
to determine a revised orbial period for HD 209458b.  Fitting an orbital
period to these 28 transit times spanning from April 2000 to August 2005 yields
a period of 3.52474832 $\pm$ 0.00000029 days.  This is in
agreement with the 2003 orbital period reported by \citet{knu07} to within
25 ms (within their 1-$\sigma$ error bars of 33 ms).  The expected drift in
the orbital
period of HD 209458b due to the first two effects in the list above over the
two-year baseline obtained when comparing our orbital period to
the 2003 period of \citet{knu07} remains smaller than the current
sensitivity.

The latter two effects on the list presented above will cause short-term
timing variations.  In terms of effect (4), we set our approach to analyzing
HD 209458 as follows.
Current Doppler radial velocity (RV) data already exclude planets with
$M > 3\times 10^{-4}M_{\odot}$ ($100$ M$_{\earth}$) and $P < 100$ days
\citep{lau05}, and at such long-period orbits RVs are
more sensitive than TTVs. This interplay between RV and TTV limits was pointed
out by Agol et al.(2005) - their Fig.7, and is likely to be common to other
bright transiting systems with good RV data (e.g., HD 189733, TrES-1, HAT-P-1).
Therefore the set of {\it MOST} transit times is particularly fit to place
limits on small close-in perturbing planets, with $P < 15$ days (or about
a third
of the length of the observing run). Despite its limitations, this is of great
interest for the HD 209458 system, because such small close-in planets could
still provide enough forcing to the eccentricity of HD 209458b for tidal
heating to occur. The same is true for systems like HAT-P-1b.

Our results show no evidence for short-term timing variations.  The
short-term scatter in the data is always below 100 s and is below 30 s for the
last 7 transits in 2005.
This imposes strong constraints on any additional planets - both in mass and
orbits.  To determine what types of planets are ruled out by the {\it MOST}
data we solved the classical N-body problem,
\begin{equation}
\frac{d^2x_i}{dt^2} = - \Sigma_{j=1;j\neq i}{N} \frac{Gm_j (x_i -
x_j)}{|x_i-x_j|^3},
\end{equation}
where for 3 bodies, x describes the initial positions of the
particles.  For the HD 209458 system, we assumed a stellar mass of 1.101
$M_\sun$ and planetary mass of 0.69 $M_{jup}$ in a circular orbit with a
period of 3.52474832 days.  A third body was inserted with an initially
circular orbit, with periods ranging from 1 to 18 days in increments of
0.01 days and masses from 1 - 100 $M_\earth$ in 1 $M_\earth$ increments, and
on coplanar orbits to HD 209458b.
The solution was advanced at 1.0 second intervals for 1000 orbits of HD
209458b ($\sim 3\times 10^{8}$ s) using the LSODA routine from ODEPACK
\citep{rad93}.  In the case where the two planets in the simulation passed
within 1 R$_{Jup}$ of each other, we determined that a collision had taken
place, and the N-body code was terminated. These orbits were deemed unstable
over the long term.  Resultant O-C values from the
simulations were calculated by a
linear interpolation to estimate the integration time when
HD 209458b returns to the midpoint of crossing the disk of the star.  Also, in
certain resonant orbits where we found that our data could limit the masses of
perturbing planets to less than an Earth mass, we ran a small number of
additional N-body simulations down to 0.1 $M_\earth$ at 0.1 $M_\earth$
intervals to determine what ranges of sub-Earth mass planets were ruled out.

To determine the expected magnitude of the TTVs, we compute a Fourier
Transform of the O-C series for each value
of period and mass of the 3rd body and extract the largest amplitude.
This is shown in Figure~\ref{JR_figure}, where we plot the TTV amplitude vs.\
orbital period, resulting from the N-body simulations.
Additionally, we compare the N-body results against all of the available
transit timing data to determine the maximum mass that an additional planet
in the
HD 209458 sytem could possess, while still remaining consistent with the data.
This allows for robust mass limits to be placed on perturbing bodies
in the HD 209458 system. We fit the combination of the 15 {\it MOST} transit
times and the 13 HST transit times \citep{ago07} to each of the O-C series
generated by the
N-body code.  This allows for a more complete coverage of the libration
period of any hypothetical 2-planet system, than fitting the {\it MOST} data
alone.  We leave a timing offset and slope as free parameters.  From this
process, we determine the maximum mass of perturbing planet that remains
consistent with the 1-sigma error bars on the transit times as a function
of the orbital period of the perurbing body, which we show in
Figure~\ref{EMR_figure}.

From Figure~\ref{EMR_figure}, we place the following constraints on the
presence of additional planets in the HD 209458 system, at the 99\% (3-sigma)
confidence limit.
First, we explore possible planets in inner orbits. Placed between
HD 209458b (at 0.045~AU) and the star, such planets are constrained to a very
narrow range of orbits. Non-zero eccentricity is a given but is also limited
for stability reasons. These orbits may be more likely due to resonant
trapping during migration \citep{zho05}, most likely at 1:2 with
P$_{orb}\approx 1.76$ d . The transit timing data limits the mass of such
planets to sub-Earth masses, $M > 0.9 \times 10^{-6}$ M$_{\sun}$
(about $0.3$ M$_{\earth}$).
If between the resonances, a planet could be as massive as 20 M$_{\earth}$
($6 \times 10^{-5}$ M$_{\sun}$) and escape detection in the transit timing
data.

Previously undetected planets in outer orbits have a larger range of possible
orbits and relaxed stability requirements on their eccentricity, compared to
the inner ones discussed above.
Nice illustrations can be found in the detailed analysis of TrES-1 by
\citet{ste05} and in Fig.\ 5 by \citet{ago05}. The {\it MOST} and HST
transit data exclude sub-Earth mass planets down to 0.3 M$_{\earth}$ in the
outer 3:2 and 2:1 mean-motion resonances,
and in the 3:1 resonance with $M > 8 \times 10^{-5}$ M$_{\sun}$
(40 M$_{\earth}$).  Outside of resonances, the {\it MOST} data limit any
planets with $P < 7$ d to $M < 17$ M$_{\earth}$ and with
$7 < P < 10$ d to $M < 100$ M$_{\earth}$. The exact limits depend on the period
of the perturbing planet according to Figure~\ref{EMR_figure}.  For orbits
with periods longer than 10 d the Doppler RV limits are better.

A range of intermediate orbits surrounding the 1:1 resonance with the
transiting planet HD 209458b
are unstable for the lowest-mass perturbers, resulting in ejections or
collisions.  Between 2.65 and 4.65-day periods we can rule out sub-Earth
mass planets due to a combination of both TTV constraints and stability
requirements.

In addition to the N-body simulations described above, we performed
a limited number of additional calculations for perturbing planets in
either mutually inclined orbits relative to the transiting
planet, or in initially eccentric orbits. For the case of a perturbing planet
on an initially circular orbit, we find that only small eccentricities
are attained (generally less than 0.1).  However, if even a small initial
eccentricity or mutual inclination between the planets is added, the resulting
orbit of the perturbing planet can attain a significantly higher mean
eccentricity over the course of 1000 orbits.  The TTV's from these
configurations therefore tend to be larger than those from the case presented
above, of a perturbing planet on a circular orbit, coplanar with HD 209458b.
Additionally, there is a smaller range of stable orbits in these cases.
There are some limited cases
however where an eccentric companion can cause slightly larger TTV's than
a planet on a circular orbit.  As another consideration, perturbing planets
starting from
different mean longitudes can result in TTV's that vary somewhat in amplitude,
where we always begin our N-body simulations with the second planet in an
orbit 90 degrees out of phase with HD 209458b.
In the absence of these exceptions, the limits that we have placed on
additional planets in the
HD 209458 system are generally robust limits across the entire range of
eccentricity parameter space, due to the fact that additional planets
residing in eccentric or inclined orbits tend to have even larger observable
effects on the transit times of HD 209458b.

\section{Summary and Conclusions}

The addition of the 15 {\it MOST} transit times to the 13 previously
available HST transit times from \citep{ago07} has allowed us to place
the tightest available limits on the presence of additional planets in
the HD 209458 system with orbital periods under 11 days.  We rule out
sub-Earth-mass planets in the inner 1:2 and 2:3
resonances as well as in the outer 2:1 and 3:2 resonances.  Super-Earths are
excluded in a range of intermediate orbits as shown in Figure~\ref{EMR_figure}.

The {\it MOST} transit timing data are unique at this time in that they have 12
consecutive transits of uniform quality and consistent photometric
precision, which is very difficult to achieve from the ground for such long
time spans. For HD 209458 these types of observations have only been
possible from space and they have not been practical with the Hubble Space
Telescope, which can only observe partial transits.  Future space-based
missions designed to look at extrasolar planets, such as CoRoT and Kepler,
will also have the ability to detect additional low-mass planets in transiting
systems via transit timing analysis. For the time being {\it MOST} serves as a
demonstration of the types of results that can be obtained from these types of
observations.

Our results show no transit timing variations on three scales: (a) no long-
term change in P since 2003 at the 25 ms level, (b) no trend in transit timings
during the 2005 run, and (c) no individual transit timing deviations above the
80 sec level. No variations on scales (b) and (c) help exclude the presence of
sub-Earth mass planets in inner resonant orbits and Earths and Super-Earths in
outer resonances and close-in ($P<10$ d) orbits.  Therefore our results
complement
previous searches for a putative longer-period planet, e.g.~the 84-day period
0.127$M_{Jup}$ perturber proposed by Bodenheimer et al.(2003). Our TTVs have
no sensitivity to detect a planet like that, but the radial velocity data has
already ruled this out \citep{lau05}.  Through a combination of the 15
{\it MOST} transit times from 2004 and 2005 along with the 13 previously
published transit times
for HD 209458b obtained in 2000 to 2003 \citet{ago07}, we have
placed the most stringent limits on additional planets in this system with
orbits between 1.5 and 10 days.

The level of orbital eccentricity of HD 209458b required to
explain its anomalously large radius ranges between 0.012 and 0.03,
given the uncertainty range for Jupiter's tidal dissipation factor, $Q_{J}$.
In order to induce such orbital eccentricity, a companion planet would either
need to be (i) significantly larger than Earth mass and in an outer orbit,
or (ii) at least Earth mass and in a mean-motion resonance with the transiting
planet.  The first of these two cases is ruled out by radial velocity data
\citep{lau05}.  The second case is ruled out by the TTV data. Hence the
problem of the radius of HD 209458b still remains, with the presence of a
sufficiently perturbing companion planet in the system ruled out and obliquity
tides remaining as an attractive alternative explanation.

Our conclusions supporting the lack of additional planets in this system
are further corroborated by the work of \citet{cro07} who use
MOST photometry of the HD 209458 system to rule out
the presence of additional {\it transiting} planets
with radii of 2-3 times that of the Earth and with periods ranging from
0.5 days to two weeks.  While such planets would need to have suitable
inclination angles to even be observed, the merit of a dual-transiting
system is that the combination of the radii of the planets (given by the
transit light curve) along with their masses (determined by their mutual
interactions as seen in the TTVs) allows for the density of both planets in the
system to be determined unequivocally \citep{hol05}.  This application of
the transit timing method could potentially allow for the first determination
of the mass and density of an extrasolar Earth-like planet, since current RV
precision cannot detect such planets.

\acknowledgements

We would like to thank Heather Knutson and Matt Holman for valuable input
into determining and interpreting transit timing variations. We would also
like to thank our referee, Eric Agol, for his very useful comments on this
paper.  JMM, DBG, AFJM,
SMR, and GAHW would like to acknowledge funding from the Natural Sciences \&
Engineering Research Council (NSERC) Canada.  RK is supported by the Canadian
Space Agency.  WWW would like to thank the Austrian FFG (project MOST) and
FWF (P17580) for funding.

redpajama_set_name: RedPajamaArXiv


text:
Bad Herrenalb è un comune tedesco di 7.530 abitanti, situato nel land del Baden-Württemberg.

Altri progetti

Collegamenti esterni

Comuni del circondario di Calw
Località termali della Germania

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text:
Nuggets Notes: Millsap, Connelly, Karnisovas, Offseason
May 22nd 2019 at 12:37pm CST by Dana Gauruder
The Nuggets are optimistic they'll retain veteran forward Paul Millsap, though not necessarily by picking up his $30.1MM option for next season, Sean Keeler of the Denver Post reports. "Our goal and Paul's goal is to have him back with us," Nuggets president of basketball operations Tim Connelly said. The easiest way to do that would be to pick up the option by the June 29 deadline but that would hamper the team's ability to make upgrades.
It already has more than $90MM in guaranteed salary commitments for next season. A more likely scenario would be to decline the option and sign Millsap to a multi-year deal in free agency at a lower annual salary. "We both want the same thing," Connelly said. "We'll figure out the best way for the organization and Paul to make sure that's achieved. I fully expect Paul to be back in a Nuggets uniform."
We have more on the Nuggets:
Connelly downplayed his interview with the Wizards for their top front office job, Mike Singer of the Denver Post tweets. "We just had a conversation. It was not much more than that," Connelly said. There are conflicting reports on whether the Wizards formally made Connelly a four-year contract offer but he ultimately decided to stay put.
Head coach Michael Malone said the organization "wouldn't have skipped a beat" if Connelly had taken the Wizards job and the Nuggets replaced him with GM Arturas Karnisovas, Nick Kosmider of The Athletic tweets. However, Malone is happy Connelly decided to stay since they and owner Josh Kroenke have a strong working relationship.
The Nuggets can't continue to rely on developing their young players alone to bridge the gap between them and the other championship contenders, Kosmider writes. The moves that Connelly makes this offseason will be crucial and viewed with intense scrutiny, Kosmider adds.
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Josh Kroenke
Tim Connelly
2 thoughts on "Nuggets Notes: Millsap, Connelly, Karnisovas, Offseason"
DXC • 8 months ago
I'd like to see AK get a chance at the top FO spot with some organization. Denver's roster is more about amateur scouting and the draft, than trades and contracts. Maybe the Knicks, after they get rid of the stooges.
x%sure • 8 months ago
"Wouldn't have skipped a beat" without Connelly? Kind of sounds like a dig. Maybe Malone agrees about AKarnisovas.

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We help you scour the universe to figure out which precious resources to sell and which to save.
A surprising amount of No Man's Sky doesn't involve simply zipping around the galaxy and staring at weird landscapes, but hunting for the resources to power and fund your trip. Here's a guide to explain each resource, what it's used for, and the best ways to find them.
There are five primary types of resources. When you scan a planet while on foot, resources will be marked on your HUD with icons. It can be a little tricky because the icons will tell you what type it is, but won't call out which specific resource it is.
And remember, if you're having trouble finding something, don't forget to talk to aliens in space stations and planetary outposts, and check the galactic trade terminal, which often has these elements for sale.
Once you have all your precious resources in tow, take a look at our other No Man's Sky guides to make some quick cash and increase your inventory size.
These are marked with a red lightning bolt, and are used to power your ship, multi-tool, and life support.
Found in all sorts of different types of plant life like trees and shrubs. If you're a monster, take out some of the local wildlife for a good carbon harvest. Be careful though, many sentinels aren't fond of you killing trees or cute mushroom people. In addition to powering your suits and multi-tool, it can sometimes be gifted to aliens in exchange for additional conversations.
You can find this in short plants on a planet's surface, but it's far easier to mine from asteroids in space in greater numbers. Whenever you're traveling between planets, take a moment to stock up. You'll burn through thamium9 easily, since it's used to charge your pulse engine and as a component in crafting certain technologies.
Found in red pointy crystals, often tall and easy to spot but sometimes just poking out of the ground a few inches. Important, since it powers your ship's launch thrusters, meaning if you've landed and you don't have plutonium, you won't be able to take off again. Luckily, it's fairly abundant on planets, especially in caves. You'll also find a fair amount in small red boxes surrounding alien outposts, so don't fret if there are no crystals in sight. Beware though, mine too many crystals and Sentinels will be scanning your tush in no time.
Marked by a yellow icon, oxides can be used in certain crafting recipes. They're also used to recharge defensive technologies like your exosuit's hazard protection capabilities and your ship's deflector shield, so it's a good idea to keep some handy just in case space pirates decide to hunt you down.
Typically found in rock formations and large asteroids, iron is one of the most abundant resources in all of No Man's Sky. Don't worry about scrapping it to free up inventory space because walking a few steps in any direction almost guarantees a method for mining iron.
You'll typically find zinc in plants with yellow blossoms, and be sure to stock up on it. It's an important ingredient in crafting warp cells, which get you from one galaxy to the next.
You can find this in yellow crystals, similar-looking to plutonium on a planet's surface. You can also collect it after destroying sentinels. It's used for recharging ship defenses and crafting upgrades for your multi-tool.
If you're looking to upgrade your existing tech, silicates will help you fashion new modules for your ship, exosuit, and multi-tool.
Look for large rock formations that stand apart from the rest of the terrain. Scanning will show you a brief holographic grid. It's not always easy to find, but when you do there tends to be tons of it.
You'll find it in blue plants, though it's not exactly abundant. It's used to create valuable ship and exosuit components, so if you have the inventory space try to keep some handy.
Look for spiky blue crystals, again, that are the same in appearance as Plutonium. Caves are a good bet. Be sure to save space for it if you can. This one is probably worth hoarding for a while since it's used for advanced blueprint crafting.
If you're looking to make bank, neutral elements are used to create valuable alloys that'll go for high prices on the galactic market, but more importantly, they're vital for crafting and repairing ship upgrades, particularly for warp drives—if you have the right recipes, that is. Either way, they're usually worth a lot on their own, so if you're trying to save up for a shiny new ride, reserve an inventory slot or two for neutrals. This section will be a bit repetitive because you can find them all in asteroids or planetside, in which case, just remember: if it shine, mine.
Your best bet for copper is in asteroids, the larger ones that take a number of shots to completely destroy. You can also find copper in floating rocks, shaped like teardrops, hovering over a planet's surface. It won't be on every planet, but if you see one there are bound to be lots more so you can stock up.
Another that can be tricky to find, but check any large asteroids you see and blast 'em until your inventory is full. Planets will have mineral towers aplenty as well.
Asteroids, asteroids, asteroids, and of course, mineral deposits on planet.
Again, asteroids are a good place to start, but you'll also find it in crystalline mineral deposits on planets too.
Find gold in asteroids or big shiny globules on a planet's surface or in the occasional—you guessed it: asteroid. Keep in mind that planets with extreme weather conditions usually harbor the rarest minerals.
Those chicken-nugget-looking things in space? Asteroids I think they're called? Shoot 'em. If you're lucky—BAM! Emeril lies in wait. If you're really lucky, it's actually a huge chicken nugget. Planetside, if you spot a lime green spire jutting into the sky, mine it.
These pretties are marked by a purple icon and are extremely difficult to find in the wild—literally. Feed animals and they might dump out a precious element. So far, all are used in high-level crafting recipes, but you can also flip them for a good price on the market or with traders.
This nets a good price in trade, but can be tough to find. Check plants, particularly those that appear to be expelling gasses.
Look for this rare element on planets with extreme climate conditions. It spawns in rocky green globules on the surface.
Found planetside, Murrine looks like a random, bulbous arrangement of golden spheres.
Very rare, and can be dropped by creatures if you feed them. It's easiest to find on the occasional trader. If you see it, clean out the stock. You know. Just in case.


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ReligionChristianityInternational
Patriarch Bartholomew will visit the United States
By Petar Gramatikov
Petar Gramatikovhttps://www.europeantimes.news
Dr. Petar Gramatikov is the Editor in Chief and Director of The European Times. He is a member of the Union of Bulgarian Reporters. Dr. Gramatikov has more than 20 years of Academic experience in different institutions for higher education in Bulgaria. He also examined lectures, related to theoretical problems involved in the application of international law in religious law where a special focus has been given to the legal framework of New Religious Movements, freedom of religion and self-determination, and State-Church relations for plural-ethnic states. In addition to his professional and academic experience, Dr. Gramatikov has more than 10 years Media experience where he hold a positions as Editor of a tourism quarterly periodical "Club Orpheus" magazine – "ORPHEUS CLUB Wellness" PLC, Plovdiv; Consultant and author of religious lectures for the specialized rubric for deaf people at the Bulgarian National Television and has been Accredited as a journalist from "Help the Needy" Public Newspaper at the United Nations Office in Geneva, Switzerland.
Ecumenical Patriarch Bartholomew will visit the United States from October 23 to November 3. His visit was postponed several times, and it remained unclear until the last moment. But it is already known that immediately after the celebration on October 22 for the 30th anniversary of his election as patriarch, he will fly to the United States.
Now the Constantinople Orthodox Church has officially announced that he will attend the opening of the church "St. Nikolai "at ground level in New York, where the assassination of the Twin Towers took place on September 11, 2001. Among the destroyed buildings was a small Orthodox church nearby.
On September 11, on the twentieth anniversary of the suicide bombings, US Archbishop Elpidophore of the Ecumenical Patriarchate lit the church's lights. It will be constantly illuminated as a symbol that "light shines in the darkness and darkness cannot defeat it," the archbishop said.
The entire program of the visit of the Ecumenical Patriarch has not been published yet, but it is known that he will meet with US President Joe Biden.
The visit is on the occasion of the centenary of the founding of the Greek Archbishopric in America in 1922. The visit coincides with the thirtieth anniversary of his enthronement. For the last time Patr. Bartholomew visited the United States twelve years ago.
#Constantinople
#Orthodox church
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It may be related to the Model 82A1®/M107®, but the M107A1 is far from a simple evolution. Driven by the demands of combat, every component was re-engineered to be lighter yet stronger. The result? A high-performance rifle that weighs five pounds less than the original M107, but is every bit as tough.
Designed to be used with a suppressor, this one-of-a-kind rifle allows you to combine signature reduction capabilities with the flawless reliability of the original Barrett M107, but with a rifle weight reduction of 5 pounds. An all new bolt carrier group has been designed and is key to making the rifle suppressor-ready. Its steel four-port cylindrical muzzle brake is engineered to work seamlessly with a quick-attach Barrett QDL Suppressor.
The lightweight aluminum upper receiver features an integrated 27 MOA optics rail. Inside the upper receiver, the bolt carrier rides on a hardened steel anti-wear strip for added durability. A thermal-guard cheek piece protects the user's face from extreme heat or cold.
Advanced design and manufacturing make the M107A1 more precise than ever. The rear barrel stop and front barrel bushing are bolted and bonded with a high strength compound. A titanium barrel key and fully-chrome-lined bore and chamber add to the rifle's durability.
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Prince Charles has called for an end to capitalism as we know it in order to save the planet from global warming.
In a speech to business leaders in London, the Prince said that a "fundamental transformation of global capitalism" was necessary in order to halt "dangerously accelerating climate change" that would "bring us to our own destruction".
He called for companies to focus on "approaches that achieve lasting and meaningful returns" by protecting the environment, improving their employment practices and helping the vulnerable to develop a new "inclusive capitalism".
The Prince was taking part in his first major UK public engagement since sparking a diplomatic row last week by likening the behaviour of Vladimir Putin, the Russian president, to Adolf Hitler.
The Prince, who has long been outspoken about the need to tackle climate change, said the world now stood at "a pivotal moment in history" ahead of major UN summit in Paris next year on reducing global greenhouse gas emissions.
"Over the next eighteen months, and bearing in mind the urgency of the situation confronting us, the world faces what is probably the last effective window of opportunity to vacate the insidious lure of the 'last chance saloon' in order to agree an ambitious, equitable and far-sighted multilateral settlement in the context of the post-2015 sustainable development goals and the U.N. Framework Convention on Climate Change," he said.
"Either we continue along the path we seem collectively determined to follow, apparently at the mercy of those who so vociferously and aggressively deny that our current operating model has any effect upon dangerously accelerating climate change - which I fear will bring us to our own destruction - or we can choose to act now before it is finally too late, using all of the power and influence that each of you can bring to bear to create an inclusive, sustainable and resilient society," he said.
The Prince was addressing an audience of 200 business leaders including Christine Lagarde, managing director of the International Monetary Fund, and chief executives of multinational companies such as UBS, GlaxoSmithKline and Unilever.
He called on businesses to focus on the long-term and make "an authentic moral commitment to acting as true custodians of the Earth and architects of the well-being of current and future generations".
"It is only by adopting a broader sense of value that our finances will be sustained and we can find new sources of profit," he said.
His comments appear to align with those of Ed Miliband, the Labour leader, who has called for "responsible capitalism".
The Prince suggested that companies must do more to put "young people properly at the heart of companies' employment practices and planning strategies, in order to tackle more effectively the world's growing youth unemployment crisis".
Businesses must also "account properly for carbon dioxide emissions, the use of water and fertiliser, the pollution we produce and the biodiversity we lose", he said.
The Prince said that businesses would be unpopular with their peers in the short term for going green but would reap "immense" rewards in the long term.


text:
Q: leaks when using jni I use valgrind to check memory leaks of a c program that invokes java method via jni. But even for the simplest program, which only creates a JVM and releases it, valgrind always reports leaks. Any suggestion?
  JNI_CreateJavaVM(&jvm, (void**)&env, &vm_args);
  (*jvm)->DestroyJavaVM(jvm);

The valgrind output:
> ==21794==
> ==21794== HEAP SUMMARY:
> ==21794==     in use at exit: 7,596,470 bytes in 1,427 blocks
> ==21794==   total heap usage: 45,668 allocs, 44,241 frees, 25,184,437 bytes allocated
> ==21794==
> ==21794== LEAK SUMMARY:
> ==21794==    definitely lost: 4,989 bytes in 24 blocks
> ==21794==    indirectly lost: 5,234 bytes in 22 blocks
> ==21794==      possibly lost: 245,199 bytes in 182 blocks
> ==21794==    still reachable: 7,341,048 bytes in 1,199 blocks
> ==21794==         suppressed: 0 bytes in 0 blocks
> ==21794== Rerun with --leak-check=full to see details of leaked memory
> ==21794==
> ==21794== For counts of detected and suppressed errors, rerun with: -v
> ==21794== Use --track-origins=yes to see where uninitialised values come from
> ==21794== ERROR SUMMARY: 4040666 errors from 332 contexts (suppressed: 4 from 4)

redpajama_set_name: RedPajamaStackExchange


text:
Cincinnati Reds rumors
Offseason-in-Review: Cincinnati Reds
A requiem for Zack Cozart.
By Cristiana Caruso@doublecee21 Mar 18, 2018, 8:28pm EDT
Share All sharing options for: Offseason-in-Review: Cincinnati Reds
Rick Scuteri-USA TODAY Sports
Cincinnati Reds (68-94)
Additions: Kyle Crockett, David Hernandez, Jared Hughes, Cliff Pennington, Oliver Perez, Ben Revere, Kevin Quackenbush
Subtractions: Bronson Arroyo, Zack Cozart, Scott Feldman, Drew Storen
Strap in kiddos because nothing is more titillating than the thrilling, exhilarating, spine-shiver-sending moves that the Reds have accomplished this winter. The only thing more fast paced than Cincinnati's front office making moves this offseason is perhaps a long distance snail race...in the Arctic tundra...and also the snails have been dead for a few weeks or so.
I have good news and bad news. The bad news is that the Reds had a pretty rough 2017 and will likely not have an outstanding comeback this season. They lost at least 90 games for the third consecutive year. Looking for a bright side is like staring at a solar eclipse head on but hey at least you'll burn your corneas out and then you never have to watch another Reds loss again.
It feels like we're grasping for straws here, but if I'm going to scrap together some good news, it's that Cincinnati wasn't completely dormant this winter and made some pretty substantial moves in the way of bullpen depth. It wasn't even close to filling all of the needs of the Reds but something is better than nothing, right...right??
One of the biggest blows to Cincinnati's hope and dream this winter was franchise short stop Zack Cozart was lost to free agency, signed away by the Angels to the tune of three years, $38 million. A moment of silence as we mourn what could have been. Anyway, back to our regularly scheduled analysis. Cliff Pennington was signed on a minor league deal and could possibly fill the Cozart gap. Top prospect Nick Senzel could also in the running for the position at short after seeing time there this spring, and maybe split the time with ultimate utility-man Jose Peraza. As of now, Phil Gosselin is slated to be the backup shortstop, but he only has five major league starts at that position. If the Reds are going to take a gamble on inexperience, they might as well do it with a player they want to mold for that position for years to come.
The Reds also did their share of cultivating minor-league deals, which felt far too in-vogue this offseason. The bullpen has been Cincinnati's biggest Achilles heel over the last two seasons, with a combined ERA of 4.65 in 2017, so the barrage of cheap reinforcement could prove to be a good investment. On the stronger part of that bolstering is David Hernandez, who inked a two-year, $5 million deal with the Reds in late January. Hernandez had a 3.11 ERA over 64 appearances split between the Angels and Diamondbacks in 2017 while striking out 52 hitters and walking just nine.
Cincinnati also signed RHP Jared Hughes to a two-year, $4.5 million deal with a club option included. Veteran pitcher and starter-turned-bullpen arm Oliver Perez was brought on with a minor-league deal and could possibly see time in the Reds' bullpen this season. Paired with 26-year old reliever Kyle Crockett that the Reds claimed off of waivers from Cleveland, Cincinnati has set up a cheap, low risk/high reward bullpen. Crockett isn't arbitration eligible for another year, so he'll be making league minimum on a strong slider as he improves the velo on his fastball.
Perhaps the only part of their roster the Reds don't have to worry about is their rotation. 2018 will be the year of the rookie starter, with young arms such as Sal Romano and Tyler Mahle competing for backend rotation slots. The offseason opened with Bronson Arroyo announcing his retirement, which was more of a hit to the team's morale than to their actual pitching strength. Arroyo went 3-6 with a 7.35 ERA over 71 innings. However, the loss is felt in the mentorship he could have provided for the slew of new pitchers set to make their debuts with the Reds this season. Anthony DeSclafani is getting rocked in spring training, so reinforcement is needed.
Ben Revere was signed to a minor-league contract and would provide nice depth for Cincy.
A big move coming from the Reds towards the end of the offseason was agreeing to terms with Eugenio Suarez on a contract extension through the 2024 season, with a team option for 2025. The third baseman is guaranteed $66 million over the next six years, with the 2025 option worth $15 million with a $2 million buyout.
The Reds didn't make a single trade this winter, and that's okay.
But Joey Votto is still around and still getting bases on balls so let's relish in that and use it to sustain us through the bad days.


Pyjama Drama themed parties, for children up to seven years, are full of drama games, music and activities which will thrill the senses and ignite the imagination.
We might be hunting for a scary dragon, flying to the jungle and swinging through the trees with some cheeky monkeys or finding out what happens when a witch on roller skates turns up at the party!
All Pyjama Drama parties combine drama, movement, music and play and every child will receive a sticker, balloon and a special birthday Pyjama Drama CD. All of our games and activities are noncompetitive – there are no 'winners' so no 'losers' either –everyone has a good time!
There are 4 age groups: Dewdrops (aged 1), Raindrops (aged 2-3), Rainbows (aged 3-5) and Sunbeams (aged 5-7). There are also a variety of themes to choose from: from 'Beep-Beep' and 'Little Bunnies' for the babies, through to 'Princesses' and 'Jungle Adventure' for the older children.
You can contact Pyjama Drama - Mirfield direct by completing the form below and clicking the 'Send' button.
These details were last reviewed by Pyjama Drama - Mirfield, MIRFIELD on 01/05/2013. NOTE: This account appears dormant. It is scheduled for deletion on or just after 02/05/2013.


text:
Q: react-native is not creating by using (expo init my-app) after installing the npm install -g expo/cli.. i am trying to use expo init my-app but it was throwing the error  Please upgrade to kleur@3 or migrate to 'ansi-colors' if you prefer the old syntax.

A: As I can see from the stack trace, you've got an ENOGIT error.

No git binary found in $PATH.

For some reasons expo needs git to initialize the project. And it tries to install react-native-maps from the git repository (not from npm).
This means you need to install git on your machine. For Windows, there is a method described here.
And your warning about the kleur is just a warning and you can simply ignore it and it is not your problem.


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Climbing aboard the Monsey bus I hand over my $9 to a lifeless looking driver. I am adorning a long skirt below my knees, thick tights and a polo neck jumper. It's 26 degrees Celsius. I brush past the dark woollen dividing curtain to sit amongst the women and prepare myself for the long haul drive in total silence. This will be my first visit to Monsey and I'm excited to see what it will bring. I am visiting a family I met through one of the women I am working with in Stamford Hill and we've agreed to meet at her house for a family portrait. She is young with 3 young children.
Instead as I arrive at the address I see a group of women with babies sitting outside in the sun. They stare at me coldly. They judge me. I ask them for help. They do not provide it. Irritated I continue searching for the house and luckily finally find my host. She greets me with utter warmth and welcomes me inside. I spend the rest of the afternoon taking pictures of her beautiful children. Monsey is place I am sure to revisit (I have returned one more time) but it will need to be in the summer. The days are too short in the winter and there s a lot of ground to cover. It's a hidden and protected community, but it has definitely caught my eye and I look forward to staying longer.


text:
Adele drops an emotional brick on the gays with 30: Despair, divorce and wine
Adele has finally dropped her long-awaited fourth studio album 30, meaning fans are once again weeping into their pillows and knocking back wine like it's going out of fashion.
The British singer released the hotly-anticipated album on Friday (19 November). The world had been waiting with bated breath for the record, which deals with the emotional destruction she felt in the aftermath of her divorce.
Most of the world will know by now that an Adele album is the perfect opportunity to wallow in your own sadness and get angry at an ex you haven't seen in six years – but 30 is also so much more than your standard break-up album.
Fans rushed to Twitter with mascara running down their cheeks to share their thoughts on Adele's magnum opus – and it's safe to the verdict is very much in favour.
Adele fans embraced their gay despair as they listened to 30 for the first time
Some fans were preparing to call a divorce lawyer after listening to the album – even though they're actually currently single.
My husband tomorrow: "good morning!"
Me after listening to #Adele one time: pic.twitter.com/lwlydDor6E
— Mike Tague (@majtague) November 19, 2021
I'm single but Adele has me ready to hire a divorce lawyer
— Rose Dommu (@rosedommu) November 19, 2021
not adele's new album making me wanna get a divorce when im not even married #adele30 pic.twitter.com/YDMALzTPcq
— ✩ (@gagasyuyi) November 19, 2021
Others were fully embracing gay despair after listening to the album – because sometimes it's better to just accept that you're trapped in Sad Girl Autumn and you can't get out.
Waking up to sad girl autumn #Adele #gay pic.twitter.com/C0f39NNdDd
— Manny Choi (@mannynotes) November 19, 2021
me and the girls and gays listening to adele pic.twitter.com/yky4GoIqWH
— sophia (@hellochaerins) November 19, 2021
A hush fell over gay twitter as a gentle rain began to fall.
The Gays told Siri to put the lights at 30% as they prepped the wine glasses and aloe infused tissues. @adele was about to drop an album, and despite the preparation, they knew they were not prepared.#Adele30 pic.twitter.com/YuQGe4lpJq
— Jeremy Crittenden (@jcritty) November 19, 2021
Some songs hit harder than others – such as "My Little Love", which features recordings of Adele speaking to her young son Angelo about how she's been having "a lot of big feelings lately".
Needless to say, people had a lot of feelings and they felt it was important to share with the group.
this literally how it feels listening to my little love #Adele #Adele30 pic.twitter.com/d7eHRYmZfU
— ًria (@chayuhri) November 18, 2021
Me after listening to the ending voice memo in my little love #Adele30 #adele pic.twitter.com/QXzn6EwPac
— Nick Hanson (@nick_hanson35) November 19, 2021
adele: *voice cracks on my little love*
me: #Adele pic.twitter.com/s88SVpyCxd
— A.J. (@ajhisnandez) November 19, 2021
Others were impressed at just how quickly Adele got to the core of the album's emotional centre – the album literally begins with the lyric "I'll be taking flowers to the cemetery of my heart".
"I'll be taking flowers to the cemetery of my heart" ADELE IT HAS BEEN FIVE SECONDS. #Adele30 pic.twitter.com/Tzhd8gtgtU
— abby (potential KE spoilers) (@villaneve15) November 19, 2021
A lot of people also related on a deep, spiritual level to "I Drink Wine", which sees Adele ruminating on how she used to soak up everything as a child – but now she just soaks up wine.
"I Drink Wine" will be looping for the next 12 months #Adele #Adele30 pic.twitter.com/LmsgJZHWHy
— Alexis Dujua (@apdujua) November 18, 2021
Even beyond the album's emotionally crushing lyrics, fans were also impressed by how different 30 sounds from Adele's previous records – many heaped praise on the singer for experimenting with new genres and for shaking things up, firmly dispelling criticisms that she's a one trick pony.
This is Adele's most experimental album in terms of sound but it's also so very well written and produced. Sonically and lyrically, it's her most honest, diverse and mature body of work. If you can't relate to at least one song, then maybe the problem is you. #Adele30 #Adele
— RoMane (@_romeko) November 19, 2021
.@Adele I asked for a new album not a life altering piece of art
— Colyn (@colynelliott) November 19, 2021
It wasn't just fans who were in love with Adele's new album either – 30 has won rave reviews, including a five star rating from Rolling Stone. The acclaimed music magazine declared that 30 is Adele's best album yet.
"Adele has never sounded more ferocious than she does on 30 – more alive to her own feelings, more virtuosic at shaping them into songs in the key of her own damn life," critic Rob Sheffield wrote.
The album also won a five star review from The Daily Telegraph, an 8/10 rating from Clash and four star reviews from the Evening Standard and The Independent, while The Guardian and NME gave the album three stars.
Adele wrote her new album to explain her divorce to her son
The album comes six years after Adele released her last record 25. The singer released "Easy On Me", the lead single from 30, in October – and the song quickly sent shockwaves through the world as Adele's remarkable, singular voice returned to the music industry after a long absence.
The song quickly skyrocketed to number one, while Adele sat down with Oprah for an in-depth interview about the heartbreaking personal difficulties she has faced since her last album was released – including the death of her father, with whom she had a complicated relationship.
In that time, Adele also divorced her husband Simon Konecki. The singer, who is now 33, separated from Konecki when she was 30 – which is why the album is named after that time in her life.
Speaking to Vogue in October, Adele explained that she wrote 30 to explain her divorce to her son Angelo in the hope that one day he will be able to go back and listen and understand what she was going through.
"I wanted to explain to him through this record, when he's in his twenties or thirties, who I am and why I voluntarily chose to dismantle his entire life in pursuit of my own happiness," Adele explained.
"It made him really unhappy sometimes. And that's a real wound for me that I don't know if I'll ever be able to heal."
The post Adele drops an emotional brick on the gays with 30: Despair, divorce and wine appeared first on PinkNews | Latest lesbian, gay, bi and trans news | LGBT+ news.
Labour MP Rosie Duffield confronted after repeatedly calling trans women 'male-bodied' on the BBC


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text:
ACTUALITY'
ARTISTS AND REVIEWS
CRAFTS AND WORKSHOPS
EVENTS AND PREVIEWS
TIPS AND TASKS
TUSCAN WINERY
TERRITORY AND TECHNIQUE
DIARY OF BUONGUSTO
IDEAS AND PROPOSALS
DISCOVER TUSCANY
Trisomy 21 Onlus, a gala evening to celebrate the 40 years of activity
The 30 November at the 19.30 in the Salone dei Cinquecento will be organized the event "Noi Abitiamo Firenze" which includes a gala dinner and a fashion show
November 27, 2019 November 27, 2019 NO PROFIT
It was the 1979 when the Association Trisomy 21 Onlus on the Florentine territory he began his activity to guarantee the respect and full rights of people with Down syndrome or similar intellectual intellectual disabilities. First in the headquarters in Via Faenza, then over the years the activity was transferred to Borgo Pinti and then to the current headquarters in Viale Volta.
Over the course of these forty years, an important job has been carried out both from the point of view of health-related qualifications aimed at achieving the maximum possible autonomy, and from the social point of view for a full inclusion, working on a network of factors that involve not only people with Down syndrome but also and above all society. The donations collected are intended to promote the social, emotional and working life of people with Down syndrome or intellectual genetic disability with the aim of achieving maximum independence, including housing. At the same time the funds are also earmarked for training and research.
To celebrate this important goal the Association Trisomy 21 Onlus has organized, under the patronage of Municipality of Florence, an event entitled We live in Florence which includes a gala dinner accompanied by a fashion show. The evening will be presented by the actress Gaia Nanni always close to the Association, and will take place in Salone dei Cinquecento in the Palazzo Vecchio il November 30 at 19.30.
"Florence chooses to host their so special birthday party in the Salone dei Cinquecento, the heart of the palace and of the city", says the councilor for Welfare Andrea Vannucci present at the presentation press conference - "It is always a very strong emotion to be able to host these guys here and hear their voices while they talk about their daily life and their work: one of them, to the question of what do you like most about her employment, he replied 'go ahead', a phrase that bears witness to a confidence, a spontaneity and a desire for the future that all young people should have. The Trisomy 21 association has been at 40 for years with these young people, providing them with support, services and above all opportunities. This is why Florence chooses to host their so special birthday party in the Salone dei Cinquecento, the heart of the palace and of the city, just as this reality is from 40 years in the heart of all Florentines ".
"It is an honor for me to celebrate the first forty years of Trisomy 21 which is, and has been, a reference point for many families, but above all for hundreds of people with Down syndrome who, thanks also to the constant support of the association, can now represent themselves and demonstrate that it is possible to occupy a place in this society sometimes too indifferent - he declares Antonella Falugiani - Even our young people represent the future of this Italy, and it is right to listen to them, listen to their needs and dreams, which are not special but are everyone's, and give it a voice. This is the responsibility of all citizens, regardless of their genetic condition. Change is underway, but we still have to fight hard for society to be fairer ".
The focal point of the evening will be the parade of clothes made by guys from the art workshop of the Association, PicEo, an important habilitative project that since 2008 has the purpose of inserting young people into the world of work. With their artifacts, in fact, the PicEo boys participate in some exhibitions such as, for example, Artigianato & Palazzo, with the aim of being able to "do business". The clothes that were made for the show are dedicated to the beauty of Florence. Walking around the center of the city, the PicEo boys discovered the lines, colors and geometric shapes of some Florentine monuments but also some symbols of Florence.
The most relevant geometries will be the marble ones of the floors and external walls of the Duomo and the Baptistery. Gold will be another important element also present in the backgrounds of the altarpiece. Color is another fundamental element. The Dutch artist Maurits Cornelis Escher wrote in his diaries that the lapis lazuli blue of the Tuscan sky had not seen him anywhere else. And then the green of the Serpentine marble of Prato, the white of Carrara marble, the red of the Siena marble trace all the facades of the most important Florentine churches. These colors, together with the blue, are found in the ancient banners of the historic districts of Florence which is nothing but an example of how many different shapes and colors create a harmonious whole.
The collection consists of hand-painted skirts with geometric patterns and dresses with designs printed on Florence interpreted by the PicEo boys. There will also be scarves, ties and accessories. For the little ones, a collection dedicated to them has been created, inspired by the animals that symbolize the city: the tortoise with the sail, symbol along with the motto Festina Lente by Cosimo I de 'Medici, the Florentine Marzocco lion and the bronze bees that are found at the base of the statue of Ferdinando I de 'Medici in piazza SS. Annunziata.
"With this initiative - he declares Antonella Falugiani - Trisomy 21, once again, tries to shake up a world closely linked to certain pre-established canons. In fact, he decided to have 40 wear non-professional models of clothes, because Beauty has endless facets. A judgment is never entirely subjective, but linked to the cultural context in which each of us is inserted ".
"I thank the Trisomy 21 Onlus Association that welcomed me into the family. The magic that made me say "I'm here" was taken to help, together with my staff, to celebrate the guys who made their projects on the fabric, creating beautiful clothes inspired by the beauty of Florence ", he comments Vivilla Zampini, Ceo Es'given, organizer of the fashion show.
The gala dinner menu was prepared by Milleluci Cafè, the bar restaurant located in Piazza Leopoldo near the Coop, managed by Trisomia 21srl, social enterprise where the guys who work on this occasion will also work in the Salone dei Cinquecento. "This is a necessary project for the path of growth and autonomy of people with intellectual disabilities - explains Antonella Falugiani - and which is useful for their social inclusion".
Both in the preparation of the menu and in the service the Milleluci Caffè boys will be assisted by the students of theBuontalenti Hotel Institute. "The involvement of a school is important for the inclusion project that concerns both the aspect of professional training but above all of relationship - continued Antonella Falugiani - and this is why we appreciated their availability, because the school is the first true aggregation moment of each person ".
"Our teachers are happy to work together with our students because we also try to pursue a path of social and professional inclusion. - he tells Rita Gaudio, support professor of the Istituto Alberghiero Buontalenti - Our students will work together with the boys of the Association for the realization of the menu and for the room service. I thank on behalf of the school manager Maria Francesca Cellai for having thought of us for the realization of this evening and the Trisomy 21 Onlus Association for the work she has done in these 40 years ".
The event will be presented by actress Gaia Nanni who has worked with the Association for many years.
"From 10 years the Trisomy Association 21 Onlus is the family that I have chosen. - comments Gaia Nanni - Trisomia did not do any assistance work but tried to include these young people in school, in the professional world, making them independent and trying to integrate them into society. I learned, if there was any need, that the desires of these boys are the same as everyone else: studying, graduating, finding a job, falling in love and getting married ".
Special thanks also go to those who supported and support the activities of the Trisomy 21 Onlus Association: Amaranto, ArteEventi, IPSSEOAB Buontalenti, Carapelli, Dini Caffè, Dori Pubblicità, Cassa di Risparmio Foundation, Ermanno Scervino, Es'Given, Eva Capelli Sartoriali, Ferragamo, Fisar Florence, Frescobaldi, Gucci, King of Truffles, Lamole di Lamole, Lito Terrazzi, Butcher Luca Menoni, Menchetti, Mercafir, Milleluci Cafè, Mukki, Pav Art, Porsche, Prelude, Prinz, Rebel, Rolando Innocenti & Figli , Salumificio Anzuini, Schema31, SGP, Stilli Solution, Tecnoservice, Land of Burchi, Thermotechnics Picchiarini, Uashmama
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Editor, graduated in modern literature and passionate about good books, theater and art exhibitions. I like to write forever.
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2007 Shortlist
Cranfield case studies
BFA visit programme
Best Factory Awards 2007 - Shortlisted Companies
The most prestigious awards and benchmarking programme in UK manufacturing has announced the final shortlisted companies.
The programme is run by Works Management in partnership with Cranfield School of Management. Since entering early in 2007, these businesses have been analysed by Cranfield School of Management, and then visited by the judging team for an in-depth review.
Those that have made it onto the shortlist are, in alphabetical order:
APPH Runcorn Landing Gear, Runcorn.
Coca-Cola Enterprises, London.
Coors Brewing, Alton.
Exception PCB, Tewkesbury.
KeyMed (Medical & Industrial Equipment), Southend-on-Sea.
Reckitt Benckiser Healthcare (UK), Hull.
Rencol Tolerance Rings, Bristol.
Rocket Medical, Washington.
Selex Sensors and Airborne Systems, Edinburgh.
Sharp Interpack, Yate.
Storm Interface, Maldon.
Ultraframe (UK), Clitheroe.
Every site is vying for the coveted Factory of the Year title, won by Vitacress Salads last year. To win overall, it must firstly win its own sector award, namely one of Best Process Plant; Best Household and General Products Plant; Best Engineering Plant or Best Electronics and Electrical Plant.
Previous entrants to the awards are eligible for the Most Improved Plant Award, and companies with less than 500 employees in the whole business for the Best Small Company.
In addition, businesses are shortlisted to be awarded for excellence in a number of key areas. These include the Supply Chain Award, the Health, Safety and Environmental Award, the People Management Award and the Innovation Award.
This year's sponsors include O2; Productivity Europe; TBM Consulting Group; Toyota Industrial Equipment; Unite the Union and Wincanton.


In the course of our work, we draw on many publications, media, and organizations.
To learn more about some of these resources, click on the links above or at right. These resources are especially useful for grantmakers, nonprofits and activists, but also for scholars and students working on narrative approaches to social justice issues.
Got a great resource you'd like us to know about? Write to us at info@workingnarratives.org and we'll take a look!


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Do Part Time Workers Get Paid Less?
How many hours is permanent part time?
Is working 32 hours a week considered full time?
Why do part time workers earn less?
Do part time employees get paid more than full time?
How much money does a part time waitress make?
How many hours do you need to work to get benefits?
What are the disadvantages of working part time?
Why is it better to work part time?
How long is a normal part time shift?
Is 32 hours considered part time?
Is 5 hours a day part time?
Is it better to work full or part time?
What rights do part time employees have?
How many hours a day is part time?
What is a good hourly wage for a part time job?
Is part time salary legal?
How much do you make a month working part time?
The Criteria For a Part-time Employee You are deemed to be a part-time worker if you are employed under these conditions: You work fewer than 38 hours each week, and.
You're a permanent employee (or you have a fixed-term contract).
A person who usually works 30 hours or more per week in their main job is considered to be employed full-time. … The United States' Bureau of Labor Statistics defines part-time employment as usually working less than 35 hours per week in all jobs. Full-time employment is defined as usually work 35 hours per week or more.
Part-time workers receive considerably lower hourly earnings than do full-time workers. … The lower skills of part-time than full-time workers result primarily from limited work experience and accumulation of human capital. Little evidence can be found of a large wage gap between part-time and full-time women.
On average, all male part-time employees receive $4.86 per hour (or 23.0 percent) less than their full-time counterparts. Female part-time employees earn an average hourly wage of $18.81, approximately the same as female full-time employees.
National AverageSalary Range (Percentile)25th75thMonthly Salary$1,875$2,833Weekly Salary$433$654Hourly Salary$11$161 more row
30 hoursIf the company is an Applicable Large Employer, an hourly employee becomes eligible for benefits if the number of hours they work meets or surpasses full-time work. The Affordable Care Act and the IRS define a full-time employee as one who works at least 30 hours a week or 130 hours a month on average.
Worker Disadvantages Part-time workers usually do not receive benefits such as health insurance, sick leave, holiday pay or vacations. When they are not working, they earn no income, which may prove detrimental during sudden illnesses or if they need to take a break.
Part-time jobs can reduce the amount of stress that you're under because you may not be given the same level of responsibility and you're able to create a better work/life balance. You're working less, so you can enjoy your venture without having to carry work around with you all day (or every day).
Part-time Employees A part time employee is a person who is employed to work less than thirty-eight (38) hours each week on a reasonably predictable basis. There is usually a minimum number of hour per shift that an employer can require a part-time employee to work (generally, it is either a minimum of 3 or 4 hours).
Is a 32-hour workload considered part-time? While most employers define full-time work as ranging between 32 and 40 hours a week, the Affordable Care Act specifies that a part-time worker works fewer than 30 hours a week on average. Under the Affordable Care Act, a 32-hour work week is considered full-time.
Answers to Questions Regarding Part-Time Positions Many part-time positions have hours ranging anywhere from 5 to 35 hours a week. The Fair Labor Standards Act (FLSA) is a federal law that mandates issues such as a national minimum wage, overtime pay, and child labor. It does not, however, define part-time employment.
They may not be as numerous as full-time employee benefits, but benefits at the part-time level can be really helpful. Balance: Instead of 40+ hours a week, many part-time jobs are between 20-32 hours a week or less. This helps to decrease the amount of stress and can create better balance between work and home.
Part-time employees are granted entitlements such as annual leave, sick leave and carers leave on a pro-rata basis according to their hours worked. Unlike casual employees, part-time workers are also guaranteed ongoing employment (or a fixed-term contract) and must give or receive notice to end their employment.
Work Hours# of hours per day# of days per weekFull time jobs8 hours per day or more5 days per week OR 3-4 days per weekPart time jobsThe average is 4 hours per dayIt depends on the job
National AverageSalary Range (Percentile)25thAverageMonthly Salary$1,625$2,209Weekly Salary$375$510Hourly Salary$9$131 more row
Under California Labor Code Section 515, most "white collar" exempt employees must "earn a monthly salary equivalent to no less than two times the state minimum wage for full-time employment." … Labor Code Section 515 does not require that an employee work full-time hours in order to be exempt.
A Part Time in your area makes on average $2,261 per month, or $53 (2%) more than the national average monthly salary of $2,209. ranks number 1 out of 50 states nationwide for Part Time salaries.
Quick Answer: Is Pass Through Income Earned Income?
What is a pass through in a house? A pass-through is
Quick Answer: What Colleges Accept A 1200 SAT Score?
Is a 1200 a good SAT score? A 1200 is an above average
Question: How Do You Wear Smart Casual?
What is the difference between casual and smart casual?
Question: How Do Beginners Make Money In The Stock Market?
How do you start putting money in the stock market?
Why Is It Bad Luck To See The Brides Dress?
What is the luckiest birth month? People born in May


In October 1993, my father, Giovanni Savo, made a career-changing decision, swapping his lifetime trade in the plastic industry for one of his great passions: motorcars. Being Italian, his appreciation of the lines and colours on vehicles is what drove his ambition to open up a panel beating and spray painting business - small enough to keep pasta on the table, but large enough to fulfil his passion for perfection. Not only did he provide a pristine finish to all his work, but his kind, generous and genuine customer service earned him a good reputation.
That is where Savo's Panel Beaters began. Sadly, Giovanni passed away in September 2001, but I continue to fulfill his legacy, and we at Savo's Panel Beaters strive for perfection in every job we undertake.


June 28, Nottingham, UK: - An unsuspecting fraudster picked the wrong piece of software to steal when he tried to purchase a product that utilises BitArts' patent pending digital fingerprinting technology using a stolen credit card. The company was contacted by the Davis County Police Department in California, who told BitArts of the fraudulent transaction and asked the company if it could help trace the transaction.
When using BitArts' software, a digital fingerprint is created during a credit card purchase transaction, which is a snapshot of the unique software/hardware identifiers taken from the PC, such as the CPU and Hard Disk IDs. This fingerprint is stored in the company's database along with details of the transaction, in accordance with data protection legislation.
During the fingerprinting process, a trace is also performed that records valuable IP details about the end user's physical location. This trace route method is powerful enough to prevent a user from blocking it and regardless of any 'alien' proxy servers that may be used it will trace the user back to their ISP.
BitArts successfully traced the transaction back to the end user with these identifiers. As a result the suspect was issued with warrants by the Davis County Police allowing them to seize the suspect's goods. The police retrieved numerous items including a PC, which were passed on to the local hi-tech crime unit who plan to use BitArts' information to locate reports on the suspect's PC for the prosecution.
A date for trial is still pending.
John Safa, BitArts Founder and CTO said: "People would consider it suspicious to walk into a bank with a balaclava on so why should Internet retailers have to endure the same anonymous threat? The only barrier in stopping credit card fraud is privacy but tell that to many credit card users who have statements littered with fraudulent transactions each month.
"The Internet might be considered to be a graveyard of defunct dot-coms but the second generation Internet is ideally suited to software distribution and license activation. The problem of credit card fraud will destroy software company revenues and indirectly cost credit card holders more as the banks absorb the price of fraud.
BitArts is a software development company that is focused primarily on the development of protection, security and encryption software providing solutions for the secure delivery of software applications and digital content, digital rights management and license management over the Internet. BitArts' suite of products incorporate the functionality for the successful management and distribution over the Internet of secure and protected software and digital content, copyright and licensing protection as well as the collection of royalties from such content.
The company was founded in 1998 by Chief Technology Officer, John Safa and now boasts an impressive management line-up which includes Danny Chapchal as CEO and Dr Sheryl Chavers, former US Undersecretary of Commerce for Science and Technology in the Clinton Administration, as Chairperson. BitArts is headquartered in Nottingham, UK with customers in more than 65 countries. BitArts has patents pending on ten core technologies, the basis of the company's unique digital security offering.


What are you favorite things to do on the weekend?
I love sleeping in, lounging around with my dog Lola, and making some something tasty for breakfast!
When it comes weekend breakfasts pancakes (vegan of course) are one of my top choices.
There's really nothing better then to sit down to a hot cup of coffee and a stack of fluffy pancakes on a cold morning.
They are also a great choice when you have people staying with you. I don't think I've ever met someone who doesn't like pancakes. Plus, it's easy to make a big batch of them if you need to feed a lot of people.
It's fun to try different topping like fruit or flavored syrups, but you can never go wrong with some classic maple syrup.
Looking for more vegan breakfast recipes? Check out Vegan Blueberry Coffee Cake, Good Morning Granola, and Instant Chai Tea Mix.
Yum, these look so light and fluffy! I'm always looking for plant-based breakfast, so I'll have to try these. Thanks!
YUM! I have recently started eating more vegan or plant-based and I am always looking for delicious recipes to try with my husband. We are super into breakfast for dinner so I am excited to incorporate this recipe in our life!
Oh these look perfect! I have plenty of vegan friends who would love them.


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My entire life I have been called a dreamer by my parents, grandparents, family, friends, co-workers and employers. For the most part, I took it as a compliment, although it wasn't always meant that way. I have been very apologetic about my dreamer ways while, continuing to traverse the country on my many adventures and shed the negative permutations of the label. Well to be blunt about it, those days are over! I've made a conscious decision to stop apologizing for who I am and live my life, as I see fit. In this blog you will find that the (insert vehicle here) part of the tag line will include: a soapbox for the occasional rant that will give you a glimpse into the things about life that cause me frustration; scribbles that will communicate my thoughts on subjects near and dear to my heart; reviews of products, services or places that I have experienced; excerpts from the book I am writing. Mostly you'll read about dreams! My dreams always have vehicles that come in many shapes and sizes: some are physical like motorcycles, boats, cars, bicycling, backpacking, hiking; even journeys into the mind to just settle ones self into a quiet day alone in a the house or a garden tub; adventures both imagined and experienced. If I dream about it, you'll likely read about it.


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Home » Sindh to rename Shaheed-e-Millat underpass after Legendary Umer Sharif
Sindh to rename Shaheed-e-Millat underpass after Legendary Umer Sharif
Celebrities, Showbiz
Murtaza Wahab, the administrator of Karachi and the spokesperson for the Sindh government, announced on Saturday that the Shaheed-e-Millat underpass in the city would be named after legendary comedian Umer Sharif, who passed away on Saturday.
"In recognition of the services rendered by late Umer Sharif, KMC will name its underpass at the intersection of Shaheed e Millat and Hyder Ali Roads as "Umer Sharif Underpass," the administrator of Karachi said on Twitter.
Umer Sharif, the legendary comedian, died in Germany at the age of 66, following a lengthy illness. He was best known for his work as a stand-up comedian.
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