text:
\section{Introduction}
Asteroseismology provides a promising avenue to determine stellar
masses.\linebreak Among the sdBs two classes of multi-mode pulsators
are known, the V361~Hya and V1093 Her stars.  The V361 Hya ones are of
short period (2--8\,min), while the V1093 Her stars have longer
periods (45 to 120\,min).  The short period oscillations can be
explained as acoustic modes ($p$-modes) of low degree $l$ and low
radial order $n$ excited by an opacity bump due to a local enhancement
of iron-group elements (Charpinet et al.\ 1997).  PG1605$+$072 (also
known as V338 Ser) was discovered to be a V361\,Hya star by Koen et
al.~(1998) and was found to have the longest periods (up to 9\,min) of
this class of stars and a very large photometric amplitude (up to
$\sim$60\,mmag).  They detected a very strong main mode together with
about 20 other modes.  The first multi-site campaign confirmed these
results and increased the number of observed frequencies to 50
(Kilkenny et al.\ 1999).  Using high resolution Keck spectra, the
stellar parameters and metal abundances were derived by Heber et
al.~(1999): $T_{\rm{eff}}=32\,300$\,K, $\log{(g
[\mathrm{g}\,\mathrm{cm}^{-2}])}=5.25$\,dex, and
$\log{(n_\mathrm{He}/n_\mathrm{H})}=-2.53$ whereas $n$ is the number
density (cgs-units are used henceforth). The small $\log{g}$ implies that
the star is quite evolved and has already left the Extreme Horizontal
Branch (EHB). Radial velocity variations due to pulsation were
detected for the first time by O'Toole et al.~(2000). We organised a
coordinated multi-site spectroscopic campaign to observe PG1605$+$072
with medium resolution spectrographs on 2\,m and 4\,m telescopes.

\section{The Analysis of the MSST Data}
During the Multi-Site Spectroscopic Telescope (MSST) campaign, we
obtained 151 hours of time-resolved spectroscopy on PG1605+072 at four
observatories in May/June 2002 (O'Toole et al.\ 2005, henceforth
Paper~I).  The spectra obtained at Steward Observatory outnumber the
data from the other observatories and are of much better S/N than the
rest of the data sets. Hence we focus mainly on the results from the
Steward data and refer to Tillich et al.\ (2007, henceforth Paper II)
for a complete analysis.  The entire data set has already been
analysed for radial velocity variations (Paper~I) and 20 modes have
been detected with radial velocity amplitudes between 0.8 and
15.4\,$\mathrm{km}\,\mathrm{s}^{-1}$.
\begin{figure}[ht!]
\centering
\includegraphics [angle=270,scale=.575,bb=302 107 554 740] {color_f1_stew.ps}
\includegraphics [angle=270,scale=.525]{multi_roy_f1_landscape_ASP.ps}
\caption{\textit{Top:} Line profile variations of the phase binned
Steward data for the strongest mode $f1$ (period P=481.74\,s). The Ca\,II
line is of interstellar nature. Its variation is due to the stellar
radial velocity correction. Besides the strong Balmer, He\,{\sc i}\ and
O\,{\sc ii}\ lines are found to vary (from Tillich et al. 2007).
\textit{Bottom:} Variations of the temperature, log $g$ (both left),
temperature and log $g$ residuals (both right) with best fit sine
curve and statistical error bars.}\label{fig_f1}
\end{figure}
As individual spectra are too noisy for a quantitative spectral
analysis in terms of detecting very small variations, they were
combined in an appropriate way.  To be able to detect tiny variations
for any pre-chosen pulsation mode, we determined the phase of each
individual spectrum according to the selected pulsation period and
co-added them weighted by S/N.  To this end, a complete pulsation
cycle was divided into twenty phase bins.  In Fig.~\ref{fig_f1}
(\textit{top}), the phase dependent changes in the line profiles of
the Steward data with respect to the mean spectrum are shown.  It is
evident that all the observed H, He~{\sc i}\ and O {\sc ii}\ lines
vary in the same way with phase.  Effective temperatures
($T_{\rm{eff}}$), surface gravities ($\log{g}$), and helium abundances
($\log{n_\mathrm{He}/n_\mathrm{H}}$) were determined for every bin by
fitting synthetic model spectra to all hydrogen and helium lines
simultaneously, using a procedure developed by Napiwotzki et
al.~(1999).  A grid of metal line-blanketed LTE model atmospheres with
solar metal abundance was used.

We start our analysis with the dominant mode in radial velocity, which
is expected to also show the largest variation in temperature and
gravity (see Fig.~\ref{fig_f1}, \textit{bottom}).  The variations of
$T_{\rm{eff}}$ and $\log{g}$ are sinusoidal. Therefore, the pulsation
semi-amplitude is determined by using a $\chi^2$ sine fitting
procedure ($\Delta T_{\rm{eff}}=873.7\pm16.5$ and
$\Delta\log{g}=0.078\pm0.003$). As expected the helium abundance
remains constant. The first harmonic is clearly recovered in the
temperature residuals (see Fig.~\ref{fig_f1} right, \textit{bottom}).
We then proceeded to search for and analyse weaker frequencies for
which
\begin{figure}[ht!]
\centering
\includegraphics [scale=.30]{multi124_oprew_stew_temp.ps}
\includegraphics [scale=.30]{multi124_oprew_stew_logg.ps}
\caption{Variations of the temperature
({\it left}) and the log $g$ ({\it right}) for the four strongest frequencies
after the cleaning procedure with the statistical error bars. The best
fit sine curves are the full drawn lines. Note that the dominant mode
is not perfectly eliminated. However the residuals are very
small.}\label{fig_f124}
\end{figure}
we developed a cleaning procedure.  First we calculated synthetic
spectra for every phase bin of the dominant pulsation frequency
$f1$. Then they were summed up to create the mean synthetic spectrum for
$f1$, which was subtracted from each phase bin spectrum to form the
cleaning function.  This correction was applied to all of the $\sim
9000$ individual spectra by subtracting the cleaning function for the
corresponding phase of the dominant mode. All individual cleaned
spectra were then summed into the appropriate phase bin for the
corresponding periods of lower amplitude frequencies (from $f2$ onwards)
and were analysed for the atmospheric parameter variations as
described above. Results are summarized in Table 1 and plotted in
Figs.~\ref{fig_f124} and~\ref{fig_weakmodes}.  Unlike the isolated
frequencies $f4$, $f2$ and $f3$ are too close together and therefore
unresolved in our analysis.  For the frequency $f9$, the errors of our
data points ($\delta
T_{\rm{eff}}=40\,\rm{K},\delta\log{g}=0.008\,\rm{dex}$) are of the
same order of magnitude as the amplitude ($\Delta
T_{\rm{eff}}=35\,\rm{K},\Delta\log{g}=0.003\,\rm{dex}$) and the
detection of variations must be regarded as marginal.  Nevertheless,
this demonstrates that it is possible to reveal variations of
atmospheric parameters of modes with radial velocity variations as
small as $2\,\mathrm{km}\,\mathrm{s}^{-1}$.  Frequencies $f5$ and $f6$ are
isolated and therefore well resolved.  By contrast frequencies $f7$, $f9$
and $f11$ are close together and therefore unresolved. While amplitude
variations of atmospheric parameters are found for $f7$, the variations
for $f9$ and $f11$ are below the detection limit.  $f8$ and $f10$ are
combination frequencies involving $f1$ ($f1$+$f5$ and $2\times f1$,
respectively). For $f8$, the variation of $T_{\mathrm{eff}}$ is detected
only marginally, whereas the gravity variation is pronounced (see
Fig.~\ref{fig_weakmodes} and Table~1).  In order to characterise
pulsation modes, it is also important to investigate the phase lags
between temperature, gravity and radial velocity variations.  These
phase lags can be used to determine the deviations from an adiabatic
change of condition.  The radial velocities of individual spectra were
taken from Paper I.

The amplitudes of their variations were determined in the same way as
the temperature and gravity variations using the phase binning and
cleaning technique described in Sect.~2. Phase lags between the
variation of radial velocity and the atmospheric parameters can be
derived directly by comparing the phases of their maxima.  In order to
determine the phase lags of the weaker modes, we used the temperature
curves, and measured just the phase lags for two sine functions.  As
the formal fitting errors are unrealistically small, we use half the
bin size ($\pm 0.025$) as error estimate.  It is worth noting that for
all recovered modes (except $f3$), the radial velocity variation reaches
its maximum before the temperature variation. Furthermore, all the
values of the phase lags lie around $0.25$($\widehat{=}\frac{\pi}{2}$)
with small but significant deviations. This is the value we would
expect for a completely adiabatic $p$-mode pulsation.
\begin{table}[ht!]
\caption{Semi-amplitudes of the temperature and gravity
variations after cleaning for the four strongest modes derived from
Steward data. Also the statistical error from the $\chi^2$ sine
fitting is listed. Periods, frequencies and radial velocity amplitudes
are taken from Paper I and therefore calculated for the whole MSST
data run.}
\centering\smallskip
\begin{tabular}{cccccc}
\tableline
\noalign{\smallskip}
Name & Period & $f$ & $v$ &  $\Delta T_{\rm{eff}}$ &
$\Delta\log{g}$ \\
& [s] & [$\mu$Hz] & $[\mathrm{km}\,\mathrm{s}^{-1}]$ & [K] & [dex] \\
&     &           &            & cleaning & cleaning \\
\noalign{\smallskip}
\tableline
\noalign{\smallskip}
$f1$ & 481.74 & 2075.80 & 15.429 &  70.5$\pm$4.7   & 0.008$\pm$0.001\\
$f2$ & 475.61 & 2102.55 & 5.372  &  132.6$\pm$12.6 & 0.011$\pm$0.002\\
$f3$ & 475.76 & 2101.91 & 2.971  &  84.5$\pm$17.5  & 0.008$\pm$0.002\\
$f4$ & 364.56 & 2743.01 & 2.497  &  140.9$\pm$14.6 & 0.011$\pm$0.002\\
$f5$ & 503.55 & 1985.89 & 2.474  &  117.9$\pm$10.3 & 0.014$\pm$0.002 \\
$f6$ & 528.71 & 1891.41 & 2.322  &  87.7$\pm$15.0  & 0.009$\pm$0.002\\
$f7$ & 361.86 & 2763.50 & 2.121  &  136.8$\pm$10.5 & 0.013$\pm$0.003\\
$f8$ & 246.20 & 4061.70 & 1.777  &  88.1$\pm$18.3  & 0.021$\pm$0.002\\
\noalign{\smallskip}
\tableline
\end{tabular}
\label{tab_pre}
\end{table}
But as a real star is a non-adiabatic system due to its radiation of
light, such deviations are to be expected.  For the dominant mode $f1$,
the phase lag between $T_{\rm{eff}}$ and $\log{g}$ is 0.3 (see Paper
II) indicating that the temperature is highest shortly after the
radius is smallest.  After that, we consider the phase lags between
the radial velocity and the gravity, which are supposed to have a
strict relationship, as they are both produced by the movement of the
stellar surface (i.e.\ the $g$ variation should be in line with the
derivative of the radial velocity curve). Hence, we expect a phase lag
of 0.25 between the RV curve and the $\log{g}$ curve.  We apply the
same fitting procedure as before. For the Steward data, most values
seem to be in agreement with the theory within
$\Delta\varphi=0.02$. This is consistent with our error estimate,
except for frequencies $f3$, $f7$ and $f8$. The difficulties with $f3$ have
already been discussed (see above) and the same may hold for $f7$ as it
is also unresolved from $f9$, whereas frequency $f8$ is close to the
detection limit (see above).
\begin{figure}[ht!]
\centering
\includegraphics [scale=.3]{multi528_prew_stew_temp_ASP.ps}
\includegraphics [scale=.3]{multi528_prew_stew_logg_ASP.ps}
\caption{Variations of the temperature ({\it left}) and the log $g$
({\it right})
for the modes $f5$, $f6$, $f7$ and $f8$ after the cleaning procedure with sine
fits and statistical error bars derived for the Steward data (from
Paper II).}\label{fig_weakmodes}
\end{figure}

\section{The Modelling of Pulsation Modes}
For the modelling we used a routine, authored and introduced by
Townsend (1997). The adiabatic code \textit{BRUCE} has been developed
to model non-radial pulsations for early-type main sequence
stars. With a radiative shell and a convective core these stars have a
similar structure as subdwarf B stars. Therefore the routines should
also be able to describe the pulsations in these smaller sdB stars.
In order to model the surface variations by a certain pulsation mode,
the stellar parameters have to be known accurately, e.g.~the polar
values for radius, temperature, gravity and inclination as well as the
equatorial rotation velocity. From these assumptions an equilibrium
surface grid of the star, consisting of 51030 points, is calculated,
taking into account any effects of the rotation on both surface
geometry and surface temperature distribution. Thereafter this grid is
perturbed by one (or several) well defined pulsation mode(s) to reveal
the temporal propagation. The perturbation must be characterized
through degree and order of a spherical harmonic and a perturbation
velocity amplitude (for more details see Townsend 1997).  The
inclination angle plays a very important role for cancellation effects
except for radial modes.  \textit{BRUCE} provides us with all the
parameters neccessary for a spectral synthesis such as temperature,
gravity and the projected values for velocity, surface area and
surface normal for every point grid point on the stellar surface.  The
\textit{KYLE} routine is based on a code authored by Falter (2001)
and used to perform the spectral synthesis for every time step.  For
this purpose it interpolates in the same grid of LTE synthetic model
spectra used for the spectral analysis (see Sect.~2) to obtain a
spectrum for every point on the stellar surface. In order to shorten
the calculation time, our model atmosphere grid was restricted to nine
points, i.e. $30\,000$\,K, $32\,500$\,K and $35\,000$\,K in
temperature and $\log{g}$ of $5.0$, $5.25$ and $5.5$. The synthetic
spectra cover $3\,000$\,\AA{} to $7\,000$\,\AA{} at a resolution of
$0.1$\,\AA{}.
\begin{figure}[ht!]
\centering
\includegraphics [angle=180,scale=0.575,bb=43 14 680 267] {color_l0m0_syn.ps}
\includegraphics [angle=270,scale=0.525]{multi_l0m0_newslow_ASP.ps}
\caption{Same as Fig.~1 but for the
synthetic line profile variations derived from our slow rotating model
{\sc i} using the same procedures as for the observed data. Note that
the first harmonic is clearly seen in both temperature and gravity at
amplitudes similar to the observed ones (compare
Fig.~\ref{fig_f1}).}\label{fig_model}
\end{figure}
Falter (2001) used a simple wavelength independent limb darkening law
in his code, which is the main drawback of this method according to
Townsend (1997). So this approximation was regarded too crude and
replaced by a quadratic law calculated for every wavelength of the
synthetic spectra. Intensity spectra for nine angels were calculated
from the model atmosphere and quadratic functions were fitted for
every wavelength.  The set of limb darkening coefficients was then
input to \textit{KYLE}.  Fig.~\ref{fig_model} (\textit{top}) shows the
theoretical line profile variation for a radial mode $l=0,m=0$ in
PG1605$+$072 calculated with the \textit{BRUCE} and \textit{KYLE}
code.  We then used the same fitting procedure described in Sect.~2 to
determine atmospheric parameters.  To complete the set of stellar
parameters we need to know the equatorial rotational velocity.  Heber
et al.~(1999) determined the projected rotational velocity to
$v_{\mathrm{rot}}\sin{i}\approx39\,\mathrm{km}\,\mathrm{s}^{-1}$ from
the observed spectral line broadening in a time integrated spectrum.
However pulsational line broadening was not considered. As the RV
amplitude of the dominant mode is large, it has to be corrected for.
Taking into account the projection factor (Montanes--Rodriguez et al.\
2001), we adopt a lower limit for the $v_{\mathrm{rot}}\sin{i}$ of
about $17.4\,\mathrm{km}\,\mathrm{s}^{-1}$.\\ Based on these
assumptions we tried two different models for PG1605+072: model {\sc
i} is a slowly rotating star with $i=90^\circ$ and
$v_{\mathrm{rot}}=17.4\,\mathrm{km}\,\mathrm{s}^{-1}$, model {\sc ii}
is a fast rotating one with $i=7.7^\circ$ and
$v_{\mathrm{rot}}=130\,\mathrm{km}\,\mathrm{s}^{-1}$. In the following
section we compare the surface variations of these very different
models.
\begin{figure}[ht!]
\centering
\includegraphics [scale=0.3] {multi_l1m+-1_newslow_ASP.ps}
\includegraphics [scale=0.3]{multi_l1m+-1_newfast_ASP.ps}
\caption{The modelled variations of the
atmospheric parameter for the mode $l=1,m=+1$ (+) and $l=1,m=-1$ (x)
with statistical error bars, sine fits and residuals for the slowly
rotating model {\sc i} (\textit{left}) and the fast rotating model
{\sc ii} (\textit{right}).}\label{fig_l1m+-1}
\end{figure}
For the radial mode $l=0,m=0$ variations in $T_{\rm{eff}}$ and $\log{g}$ do not depend on
inclination, due to the spherical symmetry of the problem.
Also the residuals show variations
of half the period attributed to the first harmonic, which have also been detected in the
observational data at very similar amplitudes. This shows the reliability of our procedure.
As can be seen from a comparison of Fig.~\ref{fig_f1} and Fig.~\ref{fig_model}, the predicted variations
for $T_{\rm{eff}}$ are much larger than observed for the dominant mode, while that of the first harmonic are
consistent with the observed ones. The predicted gravity variations however are consistent with observations
for both the dominant and the first harmonic. In their analysis of Balloon 090100001 \O{}stensen et al.\
(these proceedings) showed that the temperature variations may be strongly affected by non-adiabatic effects, while
the gravity and velocity variations are not. If we therefore rely only on the gravity variations we could conclude
that the dominant frequency is the radial mode.

For the $l=1,m=\pm1$ modes in the slowly rotating model {\sc i} we do not see a node line any more and
therefore the pattern is similar to a weak radial mode again. But now as we change sign on
$m$, the sinusoidal variation shifts with a factor of $0.5$ in phase (see Fig~\ref{fig_l1m+-1}).
The amplitudes in the slow rotating model for $l=1,m=+1$ are 1\,714\,K in $T_{\rm{eff}}$ and 0.057 in $\log{g}$,
while for $l=1,m=-1$ they are 1\,840\,K in $T_{\rm{eff}}$ and 0.073 in $\log{g}$.
Our result is that in a slowly rotating model the prograde and retrograde pulsation modes
look quite the same, in terms of sinusoidal variation, except for a phase shift of $0.5$.

In the fast rotating model {\sc ii} we view the star almost pole on, therefore we see the
node line, which divides the star into 2 areas of different size. Either the hot part or the
cold part of the star prevails and we obtain again a sinusoidal shape of the variations
with a rather low amplitude. Our modelling shows that this is true only
for the temperature variations.
For $l=1,m=-1$ we measure amplitudes of
290\,K in $T_{\rm{eff}}$ and 0.017 in $\log{g}$, while for $l=1,m=+1$ the variations are 175\,K in $T_{\rm{eff}}$
and 0.001 in $\log{g}$. Hence, for a retrograde mode the gravity variation almost disappears, while for the
prograde mode it does not.
Applying this method we derived a complete set of amplitudes for the modes $l\leq2$ (Tillich et al., in prep.).

redpajama_set_name: RedPajamaArXiv


text:
ISIS Pushes Further into Syria
By Jonathan Spyer 2015-04-10T01:32:27
In the Damascus area, meanwhile, the Islamic State is battling against a coalition of Palestinian forces supported by the Assad regime. The most significant element among the Palestinians seeking to challenge IS in Yarmouk is Hamas. The Hamas fighters in Yarmouk go under the name of "Aknaf Beit al-Maqdis." They are cooperating with the rebel Jaysh al-Islam in pro-regime forces and of course there will be no western help in that battle either.
What all this means is that while it is suffering real setbacks in Iraq, the Islamic State is at the present time not being seriously degraded, nor it is anywhere close to being destroyed (the two goals of the west with regard to the jihadis).
Rather, it is continuing to push forward in areas where western air power will not be brought to bear. It is not clear what, if any, will be the western response to this. But it shows the extent to which the western campaign in Iraq remains poorly defined and lacking in clear goals.
The various other protagonists in the single war now raging in Iraq and Syria all have clear objectives.
The Iranians want to preserve their clients in Baghdad and Damascus, and if possible to reunite these countries under their rule. Islamic State and al-Qaeda want to preserve and expand their domains. The Kurds want to hold what they have and maintain their de facto autonomous enclaves in both countries.
All of these are judiciously using the forces available to them to achieve these objectives. Only the western coalition, in a microcosm of more general western Mid-East policy, appears to be flailing, lacking clear goals and beset by confusion. The Islamic State is far from destroyed. And as it is degraded in one area, it is expanding in others.
https://pjmedia.com/blog/isis-pushes-further-into-syria/

redpajama_set_name: RedPajamaCommonCrawl


text:
export Form from './Form';
export FormBuilder from './FormBuilder';
export * as formUtils from './utils';
export * as formHelpers from './helpers';

redpajama_set_name: RedPajamaGithub


Vince Cable's pledge at the Liberal Democrats' autumn conference to work with allies to close down tax havens may not go down well with two of the party's most generous corporate donors.
Danny Alexander, the chief secretary to the Treasury, will on Tuesday announce further measures that he claims will retrieve £3bn hidden from the UK government in one European tax haven.
Alpha Healthcare and its sister company C & C Alpha Group, part of a venture capital group in the private health sector, have together donated £970,000 to the Lib Dems since 2004. Alpha's parent company, Harberry Investments, is based in a small office in Tortola in the British Virgin Islands – named as a tax haven by Congress in the US. Bhanu Choudhrie, a director in both donor companies, has also given a personal donation of £35,000 to the party. His father, Sudhir Choudhrie, who was once involved as a director of companies in the Alpha group but has now stepped down, has given a further £95,000 to the party since 2006.
The Choudhrie family, originally from India, was first introduced to the party by Simon Hughes, the Lib Dem MP for Bermondsey in south London.
Both Choudhries said in 2010 that they were domiciled outside Britain for tax purposes. If this is still the case they can, if they wish, avoid British tax on any income or gains from their overseas assets.
Contacted on Monday, one of the company's directors, Dhruv Choudhrie, declined to comment on Cable's speech, saying he was abroad. A spokesman for the company did not respond to emails or telephone calls.
Some senior Lib Dems have maintained close links to offshore havens. Lord Razzall, a former Lib Dem trade and industry spokesman, sits on the board at a firm called Ardel Holdings. The company is based in Guernsey and offers services including tax mitigation for clients, promising that "income can be rolled up tax free". Ardel helps with tax mitigation through "fiduciary structuring" for businesses and individuals. It also helps non-domiciled UK residents exploit non-taxable offshore funds.
Its website says: "The benefits and flexibility delivered by offshore companies make them a highly attractive option for clients."
Razzall said: "As an adviser to the owner of Ardel Holdings for the last 25 years I have always been satisfied that the business does not engage in activities of the type criticised by George Osborne."
The former Liberal leader Lord Steel is a non-executive director of General Mediterranean Holdings, a Luxembourg-established company set up by Nadhmi Auchi, an Iraqi-born billionaire. Steel said the company's headquarters were in Luxembourg and it held most board meetings there.
At the party's conference in Brighton Alexander will set out new resources to help tackle what he calls "tax dodgers". He will say: "With that extra effort we can recover much more from those who think they can hide their money offshore. Up to three times more – £3bn."
A spokesman for the Liberal Democrats said: "Liberal Democrats are committed to targeting companies and individuals who are using aggressive tax avoidance measures by hiding money off shore. In some cases, there are legitimate reasons for global companies to not base themselves in the UK, and even corporations such as the Guardian Media Group have on occasion used the Cayman Islands.
Regarding the donations from Alpha and C & C, he added: "They are part of global groups which have UK based businesses, paying full UK tax and employing British workers.
"But as Vince Cable and Danny Alexander have made clear, Liberal Democrats will be cracking down on anyone using tax havens to solely avoid paying a fair share of tax in the UK."


I am a strong believer that almost any trend can be interpreted in your style no matter what your age. There are some tweaks that need to happen to make something more age-appropriate, but it can always be done. This season the leather moto jacket is everywhere. This is a piece that every woman should own, and in my opinion, is timeless. Here, I've taken the same jacket and showed it at three different ages. In your 20s you can take more risks and wear a cute sequined mini to show off your legs and pair it with some killer booties. The 30s for me are really a mix; keep your cuts more flattering but take risks with color, texture and pattern like this sparkly polka dot tee. In your 40s it's all about classic shapes and pieces that flatter you. Choose colors that complement your skin tone and pop against your basics; this wool pencil skirt is the perfect example of that. Choose patterns in a smaller print that are still fun and unexpected. No matter what age you are, the biggest key to dressing on trend is confidence. Now, go pick up a moto jacket and make it your own.


text:
Q: Select a value for a Picker by tapping on the whole row I'm building a SwiftUI app that has a Picker view. It is embedded inside a NavigationView, so as I tap on the title of the Picker, I get forwarded to a fullscreen selection view to select a value. I can select one only by tapping on the Text itself, but nothing happens if I tap outside the red area.

I wonder is this an expected behaviour or some kind of a bug? Can it be fixed so tap on any part of the row will count as a selection?
The code is following:
var body: some View {
    NavigationView {
        Form {
            Section {
                TextField("Amount", text: $checkAmount)
                    .keyboardType(.decimalPad)
                // !!!
                // The picker is here
                // !!!
                Picker("Number of people", selection: $peopleIndex) {
                    ForEach(peopleRange) {
                        Text("\($0) people")
                    }
                }
            }

            Section(header: Text("How much tip do you want to leave?")) {
                Picker("Tip percentage", selection: $percentageIndex) {
                    ForEach(0 ..< tipPercentages.count) {
                        Text("\(self.tipPercentages[$0])%")
                    }
                }.pickerStyle(SegmentedPickerStyle())
            }

            Section {
                Text("$\(totalPerPerson, specifier: "%.2f")")
            }
        }.navigationBarTitle("WeSplit")
    }
}

A: Try .contentShape(Rectangle())
ForEach(peopleRange) {
    HStack {
        Text("\($0) people")
        Spacer()
    }
    .contentShape(Rectangle())
}

A: It seems that this behaviour is a bug and will be fixed in the Xcode 11.2

A: If you want to select all the row you can use an HStack with Spacer:
ForEach(peopleRange) {
    HStack {
        Text("\($0) people")
        Spacer()
    }
}

A: Hope this help you or give you some ideas.
  Picker("Number of people", selection: $peopleIndex) {
                ForEach(1..<100) { index in
                    ZStack{
                        Color.white
                        Text("\(index) people")
                    }

                }
            }

redpajama_set_name: RedPajamaStackExchange


text:
Stylos is the blog of Jeff Riddle, a Reformed Baptist Pastor in North Garden, Virginia. The title "Stylos" is the Greek word for pillar. In 1 Timothy 3:15 Paul urges his readers to consider "how thou oughtest to behave thyself in the house of God, which is the church of the living God, the pillar (stylos) and ground of the truth."
Book Note: "God's Harvard"
Hanna Rosin, God's Harvard: A Christian College on a Mission to Save America (Harcourt, 2007): 296 pp.
I picked this book up for cheap at the Green Valley Book Fair a few weeks ago while we were in between one of Sam's baseball games over in Mt. Crawford.
Hanna Rosin is a Jewish journalist who covers politics and religion for the Washington Post. Her book was written after c. a year (2006-07) spent with open access to the students, faculty, and staff of Patrick Henry College in Purcellville, Virginia. Patrick Henry is a small Christian college that primarily enrolls high-achieving students from homeschooled families. The school was founded in 2000 with the aim of creating a Christian alternative to the Ivy League. At the time the book was written—during the Bush administration—there were a disproportionate number of Patrick Henry students filling much coveted internships in the White House and throughout the corridors of power in Washington. Her book offers a glimpse into the world of the conservative Christian students at Patrick Henry and various aspects (e.g., courting, modesty issues, conservative political activism, etc.) of the "Joshua Generation" (i.e., second generation) of the evangelical homeschooling subculture. Rosin is generally sympathetic in her portrayal of Patrick Henry students and faculty. She is less sympathetic in her portrayal of Patrick Henry founder and then President Mike Farris. During the course of her year at the school, there was a major internal disruption and nine of the faculty resigned in a conflict with Farris (who since transitioned to become the school's chancellor). It sounds as though at least part of the issue was Farris' aversion to the Calvinism of some of the faculty.
One of the insights of the book, intended or not, is that there are always problems when one attempts to create a Utopia. Patrick Henry was founded as a Christian College with a strict student code of conduct, but faculty, students, and staff are all sinners. College students—even those raised in strict Christian homes—sometimes drink beer, watch restricted movies, and break the rules. Faculty members test the limits of academic freedom in a confessional school. Administrators act boorishly. Sinners act sinfully. Again, that is far from the main point of the book, but it is one message that speaks clearly.
Posted by Jeffrey T. Riddle at 11:02 AM
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After the success of last year's reissue of DESTRÖYER 666' classic Cold Steel… for an Iron Age, many fans asked for the 2000 masterpiece Phoenix Rising to get the same treatment. Well, that time has come. On August 24th (28th in North America), the Australians' sophomore album will hit the stores as CD and LP in remastered editions with brand new artwork and liner notes from the band.


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Feel free to check out these testimonials from other teachers to find out what some of their favorites are to use with students in their studios. Posted in Store, Worksheets Leave a comment Posted on December 9, 2017 by natalie As we finish out these final few weeks of 2017, I wanted to offer a small gift to all of you Music Matters Blog readers. If they were a baseball team we would compare them to New York's "Murderer's Row" in 1927, Brooklyn's "Boys of Summer" with the '52 Dodgers, or the great "Gas house Gang" from the '34 Cardinals. Posted in Music History, Practice Incentives, Store, Studio Ideas, Teaching Ideas 2 Comments Posted on August 1, 2016 by natalie Vanishing Voices: a musical race against time! Just use this code when checking out to receive 5 off: summer Posted in Fun Extras!, Store 3 Comments Posted on April 27, 2016 by natalie We are wrapping up an exciting year of expeditioning at our studio, and we have had a blast! Instead of reinventing the wheel I pulled out my tried and true Music Progressions Curriculum Guide and decided that it was just what we needed! Are you thing anything new in your studios? Print this music lesson coupon and call us today. Separate pages with enlarged blank huts so that huts may be placed in separate locations around the studio (for extra fun and adventure!) A new wall poster without huts so that the huts may be placed around the studio (this also allows more room for. I am indebted to cartoonist, Ben Lansing, author of the fabulous book, Bigwigs of Classical Music, for generously allowing me to use his composer caricatures for the Vanishing Voices theme. The coupon is good through this Saturday, June 5, so have fun shopping! Everyone who purchases the theme by tomorrow at 12:00 noon (CST) will bru coupons be entered in the drawing!


book author, trainer, and speaker.
My name is Marin Todorov and I am an independent developer and publisher. I work exclusively on iOS projects since late 2009. At present I get busy with a healthy mix of contract work, writing, developing open source software, and speaking/workshops or in-house trainings for companies.
A detailed, deep book about the Realm Database that will bring you from zero to hero!
Snippetty is a macOS application designed to assist you during live coding at conferences, webinars, or in the classroom.
Literally the book on Realm!
Literally the book on RxSwift!
My book on creating beautiful and engaging animations on iOS using Swift.
The first book on developing games for iOS using Swift. It covers the SpriteKit 2D game framework from Apple.
Tutorial book covering all newly introduced in iOS 7 APIs.
Tutorial book covering all newly introduced in iOS 6 APIs.
A blast from the past :) Tutorial book covering all newly introduced in iOS 5 APIs.
Cookbook with Adobe AIR 1.5 recipes.
EasyAnimation extends what UIKit offers in terms of animations and makes your life much easier because you can do much more without learning some perky new syntax.
SwiftSpinner shows a beautiful spinner view using the iOS animation effects for vibrancy and blur.
Automates the hum-drum data mapping for your JSON model class and features extra validation on data types and response structure.
TaskQueue helps you manage parallel or serial asynchronous tasks with ease.
I've worked on more than 15 apps - both for clients and own independently published projects.
I have a small studio called Underplot Apps. Me and my graphical artist released about 10 small apps in the first years of the app store. Some got traction and got us started on the App Store.
These days we rarely work on our own ideas, we mostly do contract work for clients if their project feels right.


My name is Umasuthan. I live with my parents. I have 2 brothers and one sister. I help at home by helping my mother. I am in Grade 6. I am currently enrolled in secondary school and my favourite subject is mathematics. I like to play ball games. I am in good health.


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text: Q: Recovering unique factorization of elements by only looking at $p^n$-th powers? I remember hearing somewhere that if $p^n$ is the largest power of a prime $p$ dividing the class number $h_K$ of a number field $K$, then there is unique factorization of the $p^n$-th powers of elements in $\mathcal{O}_K$ into $p^n$-th powers of irreducibles. I can see that there can't be any $p$-torsion for a $p^n$-th power of an ideal class (because $p^n$ is the largest power dividing $h_K$), but I'm confused as to how to translate this into a statement about factorization of elements, and why $p$ is arbitrary. Am I remembering this result correctly (if not, what is the right formulation)? Can someone provide a proof or reference?


text:
Q: The density of x_1^n+x_2^n where x_i are Gaussian We define a process $\chi_k^n=\sum _{i=1}^k x_i^n$ where x_i are iid gaussian processes.
I try to find the distribution of $\chi_k^n$. If k=1 then we get $f(x^n=y)=\frac1n y^{\frac{1-n}{n}}\exp(-y^{2/n}/2)$ and then try to do convolution but then to say something about the integral
$$C_{n}\int_{-\infty}^{\infty}\frac1n (l^2-h^2)^{\frac{1-n}{n}}\exp(-(l+h)^{2/n}/2)\exp(-(l+h)^{2/n}/2)\exp(-(l-h)^{2/n}/2)dh $$  What can I do n>2????????
Can I say somthing about the density, formula or upper bound?
Thanks.

A: Firstly you forgot to multiply the
density $f(x^n=y)$ by $1/\sqrt{2\pi}$. I think if you
obtained the density of the random variable $X_{1,2}=X_1^n+X_2^n$ by
the convolution method, the problem no more posed , because for
$X_1^n+X_2^n+X_3^n=X^n_{1,2}+X_3^n=X^n_{1,2,3}$, and you have the
density of $X^n_{1,2}$, the density of $X^n_{3}$, you can calculate
there convolution, i.e the density of $X^n_{1,2,3}$. If the calculation is
very difficult with the convolution (I think) you can
use the characteristic function. You calculate the function
characteristic of the variable $X_1^n$ that one noted
$\psi_{X_1^n}(t)$. As the two variables $X_1^n$ and $X_2^n$ are
i.i.d, then $\psi_{X_1^n+X_2^n}(t)=\psi_{X_1^n}(t)\cdot
\psi_{X_2^n}(t)=(\psi_{X_1^n}(t))^2$ and so on for
variable $X_1^n+X_2^n+...+X_k^n$ we will have
$\psi_{X_1^n+X_2^n+\ldots +X_k^n}(t)=(\psi_{X_1^n}(t))^k$. Just well calculate $\psi_{X_1^n}(t)$.


text:
Report: Eden Hazard 2.0 now set to sign new contract despite talks with Newcastle
HITC
Photo by Fran Santiago/Getty Images
According to Goal, Nabil Fekir is set to sign a new contract with Real Betis, despite holding talks with Newcastle following the Saudi Arabian takeover.
Well, after Amanda Staveley and the Public Investment Fund of Saudi Arabia (PIF) arrived, Foot Mercato claimed Newcastle spoke to Fekir.
However, it now seems as if the Frenchman won't be moving to St James' Park, as Goal believe he is close to penning a new contract.
It is said that only discussions over a release clause remain, before Fekir puts pen to paper on a new deal running until 2025.
Goal add that the France international is very happy at Real Betis, where he is considered to be a leader among the group.
The 28-year-old – who has been likened to Eden Hazard – has been a key man for Manuel Pellegrini this season, scoring three goals while also recording four assists.
Newcastle could still sign Nabil Fekir
Photo by Jose Miguel Fernandez/NurPhoto via Getty Images
It's a bit of a blow for Eddie Howe to see a target of his nearing a contract extension, although it's not all doom and gloom.
As aforesaid, Real Betis and Fekir are still in discussions over a release clause, which is one way Newcastle could lure him away from Spain.
Photo By Joaquin Corchero/Europa Press via Getty Images
Of course, it will be a task to convince the Frenchman, as he seems very happy and settled in La Liga.
However, negotiating with Real Betis wouldn't be necessary if the Magpies trigger his release clause – it remains to be seen what that sum will be.
In other news, Report: Conte wants 'special' Nuno target at Tottenham Hotspur


text:
Home » Sport » Tour of Croatia Set to Start
Tour of Croatia Set to Start
Tour of Croatia starts this month (photo credit: KL-Photo)
The 2nd Tour of Croatia international cycling race is just two weeks away…
From 19 – 24 April 2016 some of the best international riders will race on a 1,150 kilometre route along the Adriatic coast, Istria and inland Croatia over 6 stages.
This year's Tour of Croatia is one day and one stage longer than the successful first edition in 2015. Riders from 20 teams will start the race in Osijek on April 19th. The first 244 km long stage will finish in a beautiful baroque city of Varaždin. The second stage starts in a mesmerizing UNESCO's World Heritage Site National Park Plitvice and finishes in Split, Croatia's second largest city. The third leg is a bit shorter, but no slouch. It starts in Makarska and finishes after 193 km in another National Park, Krka. Stage 4 starts in Crikvenica, goes through Rijeka, Opatija and strongly finishes with a tortuous climb to Učka mountain range, one of many Nature parks in Croatia. The fifth stage is a team time trial, a 41 kilometre sprint from Poreč to Umag.
Ultimately, on April 24th, a 160 kilometre leg from Lifeclass terme Sv. Martin na Muri to Zagreb on St. Mark's square, on which the final ceremony will take place.
(photo credit: Tour of Croatia)
The race, which is classified as a first category race by the Union Cycliste Internationale (UCI), just one level below the biggest tour races such as Tour de France, Giro di Italia and Vuelta a España, will be feature some top-class riders, including Sir Bradley Wiggins, the winner of the 2012 Tour de France and the 2012 Olympic gold medallist, and also Mark Cavendish, who has won 26 Tour de France stages and is the 2011 Road World Championship. A massive TV audience is again expected, with some spectacular shots of Croatia again being beamed out to the world.
Wiggins & Cavendish
1. OSIJEK – VARAŽDIN (19.04)
2. NP PLITVIČKA JEZERA – SPLIT (20.04)
3. MAKARSKA – ŠIBENIK (21.04)
4. CRIKVENICA – UČKA (22.04)
5. POREČ – UMAG (23.04)
6. SVETI MARTIN NA MURI – ZAGREB (24.04)
You can follow the race on Tour of Croatia's official website here.
bradley wigginscyclingmark cavendishracetour of croatia
Tour de France winner confirmed for CRO Race


Karl Pilkington's hilarious global journey of self-discovery continues in this entertaining travelogue with a twist. Following his discoveries in the first series, this modern day philosopher is now turning his attention to some of life's other big issues – the body, identity, waste, art, how to live your life, and time. Embarking on an epic trip that takes him from the arctic conditions of Iceland to rural India, Mexico, Germany, across America and to the metropolis of Tokyo, the An Idiot Abroad star moans his way through a whole new series of weird and wacky experiences.