text:
\section{Introduction}
\label{sec:Introduction}
Double-lined eclipsing binaries (DLEBs) are the best known way of
accurately measuring the masses and radii of stars
\citep[see][for a recent review]{Torres_2010}.
Although recent discoveries in interferometry,
asteroseismology, and other methods provide promising new ways for
measuring stellar radii, these techniques still lack the precision of
DLEBs in almost all cases.

Comparisons of DLEBs with predicted mass-radii
relations from stellar models have been made for a variety of stellar
masses. However, until recently, only a few systems in the low-mass regime
were well characterized, mostly because of difficulties in
observing these systems. Those low-mass
systems that had been observed
showed radii consistently about 10-15\% higher than predictions from
stellar and evolutionary models \citep[see, for example][]{Torres_Ribas_2002,
Ribas_2006, LopezMorales_2007,
Ribas_2008}.
The most common explanation for this discrepancy
is that tidal
interactions in short period systems causes higher than normal
rotational
speeds, which in turn increase the level of stellar activity
\citep{Pizzolato_2003,LopezMorales_2007}.

If the above explanation for the bloated radii of the low-mass stars
is true, one would expect to find low mass
binaries that have
large separations (and periods) to have a normal
mass-radius relationship. Unfortunately, it can be
difficult to identify and observe long period DLEBs with ground based
instrumentation. K and M dwarfs can be faint, and large numbers of them
need to be monitored for long periods of time  to find eclipses.
Not that long ago, only two low mass DLEBs were known, CM Dra
\citep{Lacy_1977, Metcalfe_1996}, and YY Gem \citep{Bopp_1974,
Leung_Schneider_1978}. Recently, in the past
decade or so, various ground based
surveys have detected several more \citep[see e.g.][]{Ribas_2006,
Cakirli_2010,Bhatti_2010,Becker_2011,
Kraus_2011}.
However, nearly all of these have had short periods
of less than about
three days.  Notable exceptions include T-Lyr1-17236 with a pair of
M-stars in an 8.4 day orbit \citep{Devor_2008},
Kepler-16 with a pair of low-mass stars in a 41 day orbit
\citep{Doyle_2011},
and LSPM J1112+7626
with a pair of M-stars that are also in a 41 day orbit \citep{Irwin_2011}.

NASA's {\em Kepler} mission offers an exciting opportunity in this
field of study.  {\em Kepler} provides a virtually uninterrupted look
at roughly 156,000 stars at an unprecedented level of sensitivity.
\citet{Prsa_2011} identified 1832 eclipsing
binaries in the {\em
  Kepler} field, of which 95 have been identified from their broad-band
colors by \citet{Coughlin_2011}
as low mass (both
stars are
less than $\approx 1\,M_\odot$),
well-separated systems with deep eclipses
suited for ground-based follow-up.
We have obtained ground-based photometry and
spectroscopy of one of these candidates, KIC 6131659,
which is a long-period binary ($P=17.5$ d),
and have found that both of
the stars in KIC 6131659 are not bloated and
fit nicely on the same theoretical mass-radius relation.  This
offers support for the hypothesis that the previous observational disparity
from theory was caused by tidally induced magnetic activity.

In
\S\ref{sec:Observations} we discuss the observations, and
in \S\ref{sec:DataAnalysis} we discuss our analysis of
the data using our ELC code to model and measure
physical parameters from the observations.
In \S\ref{results} we present results,
including calculated physical parameters,
and explore how these results compare
with theoretical predictions. Finally, \S\ref{sec:Conclusion}
provides a short summary.

\section{Observations}
\label{sec:Observations}

\subsection{{\em Kepler} Photometry}

Discussions of the details of the {\em Kepler}\, mission are found
in \citet{Borucki_2010}, \citet{Koch_2010},
\citet{Batalha_2010},
\citet{Caldwell_2010}, and
\citet{Gilliland_2010}.
The {\em Kepler} spacecraft is in an Earth-trailing heliocentric orbit,
which allows for near continuous coverage of its 105 deg$^2$
field of view.  Many eclipsing binaries have been
discovered
among the {\em Kepler} targets
\citep{Prsa_2011,Slawson_2011,Coughlin_2011},
including many with periods
longer than 10 days.  We initially
selected a sample of 10 binaries for ground-based followup observations,
among them was KIC 6131659 (2MASS J19370697+4126128,
$\alpha=19^{\rm h}37^{\rm m}06\hbox{$.\!\!^s$} 98$,
$\delta=+41^{\circ}26^{\prime}12\farcs 8$, J2000).
It is relatively bright
($r=12.5$),
has a long period
(17.52 days), deep primary and secondary
eclipses (35\% and 10\%, respectively),
and has
out-of-eclipse variability at the $\lesssim 0.2\%$ level,
which is a sign that
there is little to no star-spot activity.
For this project
we obtained
the public {\em Kepler} light curves
from the MAST archive
(Kepler quarters\footnote{The {\em Kepler}
observations are divided up into Quarters of
$\approx 90$ days each, and will be denoted by Q2 for
Quarter 2, Q3 for Quarter 3, etc.}
Q0-Q6),
which include 28 primary eclipses and
24 secondary eclipses.

The {\em Kepler} data processing pipeline
\citep{Jenkins_2010a,Jenkins_2010b} outputs two types of light curves,
simple aperture photometry (SAP) light curves and ``pre-search data
conditioned'' (PDC) light curves, which have some of the instrumental
trends removed \citep{Smith_2012,Stumpe_2012}.  While recent versions
of the PDC light curves have better detrending, they still have
problems removing sudden jumps in the light curves (usually due to
cosmic rays). We have also found that the PDC process tends to
overcorrect when removing light from contaminating sources. We
therefore used the SAP data in this study, and implemented our own
detrending algorithm.  Each quarter of data is detrended
separately.
Discontinuities due to cosmic ray hits
and gaps in the light curves (usually caused by either monthly data
downloads and quarterly rolls) were identified by a visual
inspection. The light curves were then divided up into pieces using the
discontinuities and gaps as end points.  Each piece of the light curve
was normalized in a way similar to the way an optical spectrum is
normalized to its local continuum.
The relatively flat out-of
eclipse areas of the light are treated as the
``continuum'', and the
eclipses are treated
as ``absorption lines''.  Using the fitting tools in the
IRAF\footnote{IRAF is distributed by the National Optical Astronomy
  Observatory, which is operated by the Association of Universities
  for Research in Astronomy (AURA) under cooperative agreement with
  the National Science Foundation.}  task 'splot', an $n$-piece cubic
spline interpolating function (where $n$ was
typically between 10 and 30) was
fit to each piece after the eclipses were masked out using an
iterative sigma-clipper.  Each light curve piece was divided by the
interpolating function, and the normalized pieces were reassembled to
make the complete and normalized light curve.  The SAP and detrended
light curves are shown in Figure \ref{plotraw}.

There is a single point in the middle of the first primary eclipse seen in Q1 that is
much brighter than it should be, based on the other primary eclipses
seen. This outlier is believed to be a result of an error in the cosmic
ray rejection routine (J. Jenkins 2011, private communication).
A few other similar, but less deviant, outliers were identified
in other eclipses. These points were given a very low weight in the analysis described below.
Also, although the duty cycle is very high, the light curve is not complete.
A secondary eclipse was in progress during a monthly data download
in Q2, and one was in progress when the  spacecraft performed its quarterly roll at the end of Q2. Likewise in Q5, a secondary
eclipse was interrupted by a monthly data download. Since incomplete coverage may introduce errors
in the detrending, we excluded all three of these partially covered events entirely.
A complete primary eclipse was missed during the spacecraft roll after Q4, and secondary eclipses were
missed entirely during the spacecraft rolls following Q2 and Q5.

We have found that
the out-of-eclipse variability seen in the {\em Kepler}
light curves
is a good indicator
of star-spot activity.
As seen in Figure \ref{plotraw}, the out-of-eclipse variability
in the SAP
light curve of
KIC 6131659 is at a fairly low level, with a modulation
on a several day time scale
of $\lesssim 0.2\%$ of the mean flux level.
In Figure \ref{showspot}, we
compare the SAP light curve of KIC 6131659 to that of
the short-period binary KIC 11228612, which is another target in
our sample of objects for ground-based follow-up.  The
period of KIC 1122812 is 2.98046 days, and our spectroscopic results
show that the mass of its secondary is about $0.69\,M_{\odot}$,
which qualifies it as being ``low mass''.
Judging from the light curve, it appears that the rotation of
the star with the spot is roughly synchronized with the orbit, which
is not surprising
given the short orbital period.
The out-of-eclipse variability in KIC 1122812 is about a factor of
10 larger compared to that seen in KIC 6131659.
For comparison,
\citet{Basri_2011} presented a variability study of a large sample of G and M
dwarfs with {\em Kepler} data.  For stars with roughly periodic
variability, the typical amplitude of variability
seen in the light curves is
$\approx 2$ mmag, which is
similar to the level of of variability seen in KIC 6131659.

\subsection{Ground-based Photometry}

KIC 6131659 was observed on 2010 August 7
and
2011 July 6 (UT)
using the
0.6m telescope at the Mount Laguna Observatory (near
San Diego, California) and a
SBIG STL-1001 E CCD camera.  Johnson $R$ and  Kron $I$
filters
were used for the 2010 observations, and Johnson $V$, $R$,
and Kron $I$ filters were used for the 2011 observations.
The exposure times were 60 seconds for $V$, and 30 to 120 seconds
for $R$ and $I$.  A total of 109 useful images in $V$, 164 images
in $R$, and 195 images in $I$ were obtained.
Twilight flats
were taken, and dark exposures to match the exposure times of
the target images were obtained throughout the night.  IRAF was used to
make the standard corrections and calibrations
for the electronic bias, dark current, and flat-field.
The programs
DAOPHOT IIe, ALLSTAR, and DAOMASTER (Stetson 1987,
1992a, 1992b; Stetson, Davis, \& Crabtree 1991) were used
to
obtain the differential
light curves, which are shown at the top of Figure
\ref{plotLConly}, and presented in Tables \ref{Vdata}, \ref{Rdata}
and \ref{Idata}.

\subsection{Radial and Rotational Velocities}

We obtained 13 echelle spectra
using
the High Resolution Spectrograph (HRS; \citealt{Tull_1998})
and the Hobby-Eberly Telescope
(HET; \citealt{Ramsey_1998})
between 2010 August 18
and 2011 July 10 (UT).
The instrumental configuration consisted of a resolving power
of 30,000, the central echelle rotation angle, the 316 groove
mm$^{-1}$ cross disperser set to give a central wavelength of
6948 \AA, the $2^{\prime\prime}$ science fiber, and two sky fibers.
The exposure times were  600 seconds, split  into two parts
of 300 seconds each to facilitate the removal of cosmic rays.
After the electronic bias was removed from each image, pairs
of images were combined using the ``crreject'' option for
cosmic ray removal.  Spectra were extracted from the resulting
two dimensional images using the ``echelle'' package in IRAF.
In this study we used the spectra from the ``blue'' CCD,
which provides a wavelength coverage between about 5100 and
6900 \AA.
The data are generally of high quality, with signal-to-noise
ratios on the order of 100 per pixel near the peak
of the blaze functions.

Each night, one of
several stars with precise radial velocities taken
from the catalog
of \citet{Nidever_2002}
were observed by the HET staff using the same instrumental configuration
used for the KIC 6131659 observations.
We have a total of 77 spectra of 40 bright mostly G-type
stars from our program (including ones from
nights when KIC 6131659 was not observed), and using
simple cross correlation near the Mg b
features we found that the spectrum of the G5V star
HD 135101 provided the best match (Figure \ref{plotspec}).

The radial velocities were measured using
the ``broadening function'' technique developed by
\citet{Rucinski_1992,Rucinski_2002}.
The broadening functions (BFs) are  rotational
broadening kernels, where the centroid of the peak yields
the Doppler shift and where the width of the peak is
a measure of the rotational broadening.  For double-lined
spectroscopic binaries the BFs generally provide better
radial velocity measurements than cross-correlation measurements
made with a single template star, especially in cases
where the velocity separation of the two stars is close
to the velocity resolution of the spectra.
See \citet{Bayless_Orosz_2006} for details of this process as
applied to similar HET spectra.
As a check
on the process, we measured the radial velocities
of all of our standard star observations using
the IRAF task fxcor (a cross-correlation routine with
a single template spectrum)
and using the BFs, where the spectrum of
HD 135101 was used as the template in both cases.
A comparison
of the BF minus fxcor radial velocities shows a median difference
of 0.004 km s$^{-1}$ and an rms of 0.061
km s$^{-1}$.  The rms of the differences is comparable to the
typical uncertainties in the radial velocity measurements
reported by fxcor.

We derived BFs for all 13 observations of KIC 6131659 using
HD 135101
as the template star, whose
heliocentric radial velocity was taken to be
$-38.921$
km s$^{-1}$  \citep{Nidever_2002}.
We found that
the derived radial velocities are very insensitive to the
spectral type of the template as
similar
results were obtained using the other
(mainly) G-type radial velocity standard stars and from using
a spectrum of 61 Cyg A (spectral type K5V).
Figure \ref{plotBF} shows four example BFs.
Since care
was taken to observe near the quadrature phases, we
see well-defined peaks corresponding to the primary and
secondary stars.  In every case, there is a third peak located
between the primary and secondary peaks, which occurs at
roughly the same heliocentric velocity.
For each observation,
we compared the BF derived from the sky-subtracted spectrum to
the one derived from a spectrum with no sky subtraction and found
little, if any change.  Also, the BFs of other targets in
our sample observed with the same instrumentation show
no third peak.  Thus
we believe this third peak is real and is due to a faint
star.

The BFs were fit to a model consisting of three Gaussian
functions\footnote{For cases where the width of the BF peak is
similar to the velocity corresponding to a resolution element,
a Gaussian is often a better model than the standard
analytic broadening kernel (Gray 1992).}
to determine the centroids and widths of the
peaks.
All of the points in each BF were given equal weight, and formal errors
on the centroids were found by scaling the uncertainties to give
$\chi^2_{\nu}=1$.
By doing this, the
resulting radial velocities derived from
the peak centroids (Figure \ref{plotRVonly})
have formal uncertainties of typically 0.05 km
s$^{-1}$ for the primary and 0.45 km s$^{-1}$ for the secondary,
respectively.
The full width at half maximum (FWHM) of the
primary and secondary peaks in the BFs are approximately
10 km s$^{-1}$,
which is similar to the spectral resolution.  Thus the
stellar
rotational velocities $V_{\rm rot}\sin i$
are not resolved in our observations
and are less than about 10 km s$^{-1}$.

The BFs of the third star are well separated from the BF peaks of the primary and
secondary star.  Thus the radial velocities of the primary and secondary should
not be biased by the third star. Also, the radial velocities of the third star
are roughly constant and there is no indication that the third star
interacts with the binary.  Thus, it is sufficient to model the radial
velocities of the primary and secondary with a standard binary star model.
In this case, we modeled
the radial velocities for the primary and secondary
using a double-sine model where the sines have a common
period
and systemic velocity and phases 180 degrees apart
(the use of a double sine model is justified since
we show below that the eccentricity is essentially zero).
The uncertainties
on the individual measurements were scaled to give $\chi^2_{\nu}\approx 1$ for
each curve separately.  The resulting median uncertainties are
0.45 km s$^{-1}$ for the primary and 0.57 km s$^{-1}$ for the secondary,
respectively.  Figure \ref{plotRVonly} shows the velocities
and the best-fitting models.  The final adopted radial velocity
measurements with the scaled
uncertainties are given in Table \ref{RVdata}, and the
spectroscopic orbital parameters are given in
Table \ref{specparm}.

The HET's HRS used at resolution
$R=30,000$ can yield radial velocities with
very small errors on sufficiently bright stars,
provided that ThAr comparison lamp spectra are obtained in
a bracketing fashion, both before {\em and}
after observations of celestial targets, to detect and
correct for ``settling'' of the cross-disperser grating
following configuration changes (S. Mahadevan 2011,
private communication).  Configuration changes
are frequent, since the HET is used in a queue-scheduled mode.
In our program, however, ThAr lamp observations were often obtained
only before {\em or} after observations of a target.

As noted before we have 77 observations of 40 bright stars in our
program.
We established a grading scale to quantify the stability of the
HRS cross-disperser during the observation of the standard stars
and their associated ThAr arc exposures, based mainly on the length
of time between the configuration change and the actual
observations.  Nineteen observations were deemed to be
trustworthy in the sense that there probably was enough
time for the cross disperser to settle before the
standard star observation (our best-matched template
star HD 135101 is included in that sample).  In most of these
cases there was an observation of a rapidly rotating B-star
or other type of calibration observation just after
the configuration change and before the standard star observation.
Using HD 135101 as the template, we measured the radial velocity of
the other 18 stars in this sample and compared the measured
velocities with the velocities from the catalog of
\citet{Nidever_2002}.   Although this catalog does not give uncertainties
on the individual velocities, the rms scatter of multiple measurements
for each star is reported to be less than 100 m s$^{-1}$.
A histogram showing the distribution
of radial velocity differences
is shown in Figure \ref{OCRV}.
The median difference is 0.069 km s$^{-1}$
and the rms is 0.157 km s$^{-1}$.
The distribution can be fit by a Gaussian with
a $\sigma$ of 0.130 km s$^{-1}$.
Based on this analysis we conclude
the zero-point of our
velocity  is consistent with
the scale
defined by the \citet{Nidever_2002} catalog.  Furthermore,
based on the spread of the radial velocity
residual values,  the floor on the
uncertainties
of individual velocity measurements is
$\approx 0.16$ km s$^{-1}$.

The radial velocities of the third star show no obvious trend.
The median heliocentric velocity of the third star is 10.74 km s$^{-1}$,
and the rms of the 13 measurements is 0.83 km s$^{-1}$.  This median
velocity is  close to the systemic velocity of the binary,
which is $\gamma=8.142\pm 0.008$ km s$^{-1}$, where the uncertainty
does not include the error in the velocity zero-point.
When one considers the
velocity dispersion
of stars in the solar neighborhood, which is anywhere between $\approx 20$
and 60 km s$^{-1}$,  depending on the age
\citep{Nordstrom_2004}, the chance that two random stars will have a radial
velocity within $\approx 3$ km s$^{-1}$ of each other is somewhat small.
Also, a wide, hierarchical triple with an outer period of several years could have
a velocity difference of a few km s$^{-1}$, so it is tempting to conclude
the third star is bound to the eclipsing binary.
However,
the modeling results presented below seem to suggest
that the third star is not related to the binary.

\subsection{Metallicity and Effective Temperatures}

Accurate temperatures and metallicity are essential for the
characterization of both stars, but our photometric data does not
provide strong constraints on either parameter. The eclipses observed
in the light curve yield the {\em ratio} $T_{{\rm
eff},2}/T_{{\rm eff},1}$, but only weakly constrain the absolute
temperatures, and the metallicity cannot be reliably determined
photometrically. A spectroscopic analysis can determine the effective
temperature, surface gravity, and metallicity, but all three
parameters are highly correlated and the results are unreliable in the
absence of external constraints. In eclipsing systems the surface
gravities can be determined from the light curve, effectively reducing
the problem to a more manageable $T_{\rm eff}-{\rm [m/H]}$
degeneracy. Similar to the spectroscopic analysis of Kepler-34 and
Kepler-35 \citep{wel12}, we employed the two dimensional cross-correlation
routine TODCOR \citep{Zucker_1994} and its extension into three dimensions
TRICOR,
along with the Harvard-Smithsonian Center for
Astrophysics (CfA) library of synthetic spectra to determine the
effective temperatures of the binary members and the system
metallicity.

The CfA library consists of a grid of Kurucz model atmospheres
\citep{kur05} calculated by John Laird for a linelist compiled by Jon
Morse. The spectra cover a wavelength range of $5050-5360$ \AA, and
have spacing of $250$~K in $T_{\rm eff}$ and $0.5$ dex in $\log g$ and
[m/H]. Initially, TODCOR was used to get the parameters for the primary
and secondary.  To do this,
we cross-correlated the HET/HRS spectra with every pair of
templates spanning the range $T_{{\rm eff},1}=[4000,6500]$, $T_{{\rm
eff},2}=[3500,6000]$, $\log g_{1,2}=[3.0,5.0]$, ${\rm
[m/H]}=[-1.5,+0.5]$, and recorded the mean peak correlation
coefficient at each grid point. Next, we interpolated to the peak
correlation value in each parameter (but fixed the surface gravities
to those found from the photometric analysis) to determine the
best-fit parameters for the binary.
After the initial TODCOR fits, the third star was accounted for
using TRICOR, which yielded improved  parameters for the stars
in the binary.
Given the coarseness of the
template grid, we assigned internal errors of $100$~K in $T_{\rm eff}$
and $0.20$ dex in [m/H]. As mentioned above however, the degeneracy
between temperature and metallicity could cause correlated errors
beyond those quoted here. We explored this by fixing the metallicity
to the extremes of the $1$-$\sigma$ errors and assessing the resulting
temperature offset. Incorporating these correlated errors, we report
the final parameters for
KIC 6131659:
$T_{{\rm eff},1} = 5660 \pm 140$~K,
$T_{{\rm eff},2} = 4780 \pm 105$~K, ${\rm [m/H]} = -0.23 \pm 0.20$
dex. The calculated light ratio in the wavelength range used in the
analysis ($5150-5360$ \AA) was $L_2/L_1 = 0.105 \pm 0.004$.
The derived radial velocities were consistent with those
derived using the BF analysis, where $K_{1,{\rm TRICOR}}
=40.95\pm 0.18$ km s$^{-1}$ and $K_{2,{\rm TRICOR}}=
54.90\pm 0.22$ km s$^{-1}$.

The temperature, gravity, and metallicity of the third star
are not well constrained by the TRICOR analysis.  The third
star contributes relatively little to the fits, and similar
correlations were found even when the temperature and
gravity of the third star were changed by several grid points.
In the end, values of $T_3=5000$~K, $\log g_3=3.5$, and
$[m/H]_3=0$ were adopted for the final TRICOR runs.

\section{Light Curve Modeling}
\label{sec:DataAnalysis}

\subsection{Overview}

We use the ELC (Eclipsing Light Curve) code \citep{Orosz_2000} to model
the light curves.  ELC normally uses the standard Roche geometry to specify
the shapes of the stars, and uses specific intensities from model
atmospheres.  The stellar surfaces are divided up into tiles, and
the flux is obtained by numerical integration.  When fitting high
signal-to-noise light curves such as those provided by {\em Kepler},
one obviously needs high precision models, and this is
usually done by using more tiles over the stellar surfaces.  However,
the computational
time needed to fully sample parameter space becomes prohibitive,
so for well-detached binaries
such as KIC 6131659 where the stars are very nearly perfect spheres,
another mode of operation was added to ELC where the
analytic expressions developed by \citet{Kopal_1979},
and revisited
by \citet{Gimenez_2006}, are used to compute the light curves.  Those equations
are a function of the fractional radii of the two stars, the inclination,
the limb darkening coefficients, and the orbital phase.  For each star,
the specific intensity at the normal (i.e.\ at $\mu=1$) is taken
from the model atmosphere table for the appropriate temperature and gravity,
and intensities for other angles are computed from the limb
darkening law, which is either the linear
[$I(\mu)=I_0(1-x(1-\mu)$]
or the ``quad''
[$I(\mu)=I_0(1-x(1-\mu)-y(1-\mu)^2)$]
law.
ELC's ``analytic'' mode has the advantage in that it is very fast, and
large swaths of parameter space can be explored in a relatively short
time.  The disadvantages are that
other effects, such as
reflection, ellipsoidal
variations, and star spots
cannot be easily modeled.

In order to fully match the {\em Kepler} long cadence (LC) data,
the model light curve is computed at phase intervals that
correspond to roughly 1 minute. The model {\em Kepler}
curve is then binned using simple numerical integration
to a bin size of 29.4244 minutes \citep{Gilliland_2010}.  Such binning
is absolutely necessary as the shapes of the model eclipse profiles
change noticeably.  Since the ground-based light curves are measured
using images with much shorter exposure times, no binning is applied
for them.

For KIC 6131659, we used a model with 24 free parameters.
The inclination $i$, mass ratio $Q=M_2/M_1$, the $K$-velocity
of the primary, and the orbital period $P$
set the scale of the binary (e.g.\ the semimajor axis
$a$ is uniquely determined).  The shape and orientation
of the orbit is set by the
eccentricity $e$, the argument of
periastron $\omega$, and a reference epoch, which we take to be the time
of the primary superior
conjunction $T_{\rm conj}$.  The fractional radii $R_1/a$ and $R_2/a$
set the sizes of the stars.  The stellar temperatures are determined by
specifying the primary temperature $T_1$ and the temperature ratio
$T_2/T_1$. For KIC 6131659, we have two external
sources of contaminating light.  There
is light from the  star noticed in the spectroscopy (and possibly physically
associated with the binary) which contaminates all
of the light curves.  This third light is parameterized by the
temperature $T_3$ and a scaling factor $S$, which is the ratio
of the projected area of the third star to the projected area of
the primary.
There is also contaminating
light in the {\em Kepler} light curve from stars on the sky whose
light leaks into the KIC 6131659 aperture.
According to the
Kepler Input Catalog, the fraction of light from other sources is
a few percent.
Since the {\em Kepler} pixels are relatively
large, the stars that contaminate the {\em Kepler} light curve
are not a problem for ground-based observations, so a correction
is applied only to the model {\em Kepler} light curve.
The
parameter $k$ gives the fractional
level of contamination, and the modified flux
$f_{\rm new}$
at each phase is given by
\begin{equation}
f_{\rm new}=f+{kf_{\rm med}\over 1+k}
\end{equation}
where $f$ is the model flux before correction, and  $f_{\rm med}$
is the median flux of the entire model light curve before correction.
Finally, we have two limb darkening coefficients for each star for
each bandpass.  However, since the secondary eclipse is not observed
in the $V$,
$R$ and $I$ light curves, we don't fit for those coefficients.
This leaves us with a total of 10 coefficients:  $x_1(K)$ and $y_1(K)$
for the primary in the {\em Kepler} bandpass,
$x_2(K)$ and $y_2(K)$ for the secondary
in the {\em Kepler} bandpass, $x_1(V)$ and $y_1(V)$ for the primary in $V$,
$x_1(R)$ and $y_1(R)$
for the primary in $R$, and $x_1(I)$ and $y_1(I)$ for the primary in $I$.

\subsection{Combined Long Cadence Data Fits}

ELC's genetic algorithm
and its Monte Carlo Markov Chain were
both used to optimize the model fits to the LC data.  Generally speaking, the parameters
were allowed to vary over relatively wide ranges.  The fits
are not sensitive to the adopted value of the primary temperature.
Based on the spectral type of around G5V and on the TODCOR
analysis, we adopted a range
of $5460 \le T_1\le 5860$ K.
After some initial runs it was apparent that there was some difficulty
with the relative weights between the radial velocity curves and the light curves.
Solutions would often converge where the radial velocities were not optimally
fit.
Some experimentation showed
that the optimization worked better
when the radial velocity curves were decoupled from the
light curves.  Thus
we fit only the photometric data, using the usual $\chi^2$ statistic
as the fitness function:
\begin{eqnarray}
\chi^2_{\rm photo}
&=& \sum_{i=1}^{23123}{(f(\phi_i;\vec{a})-f_{\rm obs}(K))^2\over \sigma_i^2}
\nonumber \\
&+& \sum_{i=1}^{109}{(f(\phi_i;\vec{a})-f_{\rm obs}(V))^2\over \sigma_i^2(V)}
\nonumber \\
&+& \sum_{i=1}^{133}{(f(\phi_i;\vec{a})-f_{\rm obs}(R))^2\over \sigma_i^2(R)}
\nonumber \\
&+&  \sum_{i=1}^{162}{(f(x_i;\vec{a})-f_{\rm obs}(I))^2\over \sigma_i^2(I)}
\end{eqnarray}
where $f(\phi_i;\vec{a})$ is the model flux at a given phase $\phi_i$ for
a vector of parameters $\vec{a}$, $f_{\rm obs}$ is the observed
value at the same phase, and  $\sigma_i$ is the uncertainty.
The uncertainties on the measurements were scaled to give
$\chi^2\approx N$ for each data set separately.  The resulting median
uncertainties are 0.000089 mag, 0.0076 mag,
0.0070 mag, and 0.0090 mag for the {\em Kepler}, $V$, $R$, and $I$-band
light curves, respectively.
The component masses were forced
to be consistent with the values found from the separate fits to
the radial velocity curves by means of additional
$\chi^2$ penalties:
$$
\chi^2_{\rm RV}=(M_1-0.922)^2/0.007^2+(M_2-0.685)^2/0.005^2.
$$
The fitness function used  for a given model was
$\chi^2_{\rm tot}=\chi_{\rm photo}^2+\chi_{\rm RV}^2$.
Roughly 2.2 million  models were computed from
runs of the genetic and Markov chain codes to arrive at the
optimal model.  The uncertainties on the fitted parameters
and derived astrophysical parameters were arrived at by marginalizing
the $\chi^2$ hypersurfaces over the various parameters of interest.
The best-fitting models are shown in Figure \ref{plotLConly}
and the parameters
are summarized in Table \ref{lightparm}.
The orbital eccentricity is small, but differs from zero.
Since the argument of periastron $\omega$
and the eccentricity $e$
are
highly correlated, we give the quantity $e\cos\omega$
in Table \ref{lightparm}.
The contamination in the {\em Kepler} light curves due to other
light sources leaking into the aperture
is found to be zero within the errors.

\subsection{Long Cadence Fits to Individual Eclipses}

Figure \ref{plotresiduals} (top panels)
shows the residuals from the combined
Q0-Q6 fit for both the primary eclipse and secondary eclipse.
The scatter in the out-of-eclipse regions is somewhat smaller
than the scatter in the eclipse phases, which suggests that
there may be some
small systematic errors.  As a check on these systematic issues,
we divided the
{\em Kepler} light curve into
24 segments, each containing
a pair of primary and secondary eclipses.    Each segment was
paired with the ground-based $V$, $R$ and $I$ light curves
and modeled separately.  Figure \ref{plotresiduals}
(bottom panels)
shows
the stacked residuals from all 24 fits.  In this case the scatter
in the in-eclipse and out-of-eclipse phases is similar.
Evidently there are small changes from eclipse to eclipse,
perhaps caused by small star spots being eclipsed, errors
in the light curve normalization, or changes in the contamination level
from Quarter-to-Quarter, or all three.  The change to each
eclipse profile is relatively minor and can be fit for
by small changes in the fitting parameters such as
the inclination or fractional radii.
Table \ref{lightparm} gives the mean,
minimum and maximum of each free parameter over the 24 segments,
as well as the rms.  Figure \ref{plotspread} shows the individual values
plotted as a function of time for eight fitted and derived parameters.
In most cases, the rms of the individual values from the 24 segments
is a bit larger than the formal $1\sigma$ error derived from the combined
{\em Kepler} light curve, which might be an indication that the formal
uncertainties on the values derived from the combined fit are too small.
We note that
although the fits to each segment are
not completely independent owing to the inclusion of the same
ground-based data in each one, the spread in the resulting
best-fitting parameters that are strongly constrained
by the {\em Kepler} data, such as the inclination or the fractional
radii, should give us some independent measure of the
uncertainties.   For our final adopted parameters, in most cases
we adopt the values found from the median of the 24
individual segment fits, and adopt the rms in those
24 values as conservative $1\sigma$ error.  By doing this,
for the vast majority of the cases,
the difference between the parameter
value derived from the combined Q0-Q6 light curve
and the median value found from the individual segments
is less than
$1\sigma$,
using the rms as that uncertainty.

\subsection{Fits to Short Cadence Data}\label{SC}

There is one month of short cadence (SC) data \citep{Gilliland_2010}
for KIC 6131659 publically available, namely from the first month of
Q5.  One primary eclipse and two secondary eclipses are covered.
As noted above, the SC data cannot be modeled simultaneously
with the LC data owing to the vastly different ``exposure times''
(i.e.\ 58.85 seconds vs.\ 29.4244 minutes).  Thus the SC data
were treated as one of the individual segments discussed above
and modeled with the ground-based light curves.  Table
\ref{lightparm} gives the parameters.  For the most part there is
very good agreement between parameters measured from the SC data,
the combined LC data, and the individual segments of LC data.

One interesting thing to note about the SC fits is that the
eccentricity is  small,
but is distinctly different from zero:
$e\cos\omega=(6.88\pm 0.02)\times 10^{-5}$.
Fits with the eccentricity fixed at zero (i.e.\ circular orbit models)
gave significantly worse fits.
Figure \ref{SCresiduals} illustrates the situation.
The top panels
show the folded SC data and the best-fitting models
of both the primary eclipse (left panel) and secondary (right panel).  The
middle panels show the residuals of the fits for the primary
eclipse (left panel) and the secondary eclipse (right panel), and there
is a small scatter with an rms on the order of 1 mmag, and no apparent
features near the eclipse phases.  On the other hand, the residuals
from the circular orbit model have distinctive features near the
eclipse phases (bottom left for the primary eclipse and bottom
right for the secondary eclipse).  The phase difference between the primary
and secondary eclipse for the eccentric model is 0.500044, or about
67.2 seconds late compared to phase 0.5.

The delay in the secondary eclipse
relative to phase 0.5 is due to a combination
of light travel time across the orbit and
geometry in a slightly eccentric orbit
where the true anomaly is not equal to the mean anomaly.
The time delay due to light travel time is given by
\begin{equation}
\Delta t_{\rm LT}={PK_2\over \pi c}\left(1-{M_2\over M_1}\right)
\end{equation}
where $c$ is the speed of light \citep{Kaplan_2010}.
Substituting the appropriate
numbers from Table \ref{specparm}, we find $\Delta t_{\rm LT}=23.1$
seconds.  Thus
the delay due to light travel time is roughly one third of the
measured delay.
The change in the relative timing of primary and secondary eclipse is given
by
\begin{equation}
\Delta t_e\approx {2Pe\over\pi}\cos\omega
\end{equation}
\cite{Kaplan_2010}, where a factor of two correction has been applied to his
Equation (6).
Using values in Table \ref{lightparm}, the above approximation yields
$\Delta t_e=66.4$
seconds, which is
very close to the value of 67.2 seconds
we measured using the short cadence data.
Accounting for light travel
time, the true delay is
$\Delta t_{e,{\rm cor}}=44.1$ seconds.
This then gives
$e\cos\omega=4.57\times10^{-5}$.
Lucy (2012) recently discussed the process of
setting upper limits on the eccentricity where a Bayesian prior
on expected tidal evolution of the eccentricity is included.
Binaries where $e\ll1$ but $e\ne 0$ are occasionally expected
to occur.

\subsection{Discussion of Third Light}

We have two distinct parameterizations of third light.
The {\em Kepler} contamination parameter
$k$ accounts for other unrelated stars that are inside the {\em Kepler}
photometric aperture, but {\em not} inside any ground-based apertures.
As we discussed earlier, $k$ is very close to zero.
The quantities $S$ and $T_3$ are used to characterize light from a third
star that is present in {\em all}
of the light curves.  There are strong and compelling
reasons for including such a star, chief among them the fact that a third star
was noticed in the spectra.

Regarding the parameters for that third star noticed in the spectra,
the scaling parameter
$S$ and the third light temperature $T_3$ are somewhat anti-correlated.  However,
the combined effect of these parameters is
such that the amount of light from the third star is roughly equal
to the amount of light from the secondary star.
This rough equality between the two
is consistent
with what is seen in the broadening functions
(Figure \ref{plotBF}).
The value of the parameter $S$ indicates the third star's
{\em angular} radius is between $\approx 44\%$---$55\%$ the
{\em angular} radius of
the primary.  For comparison, the angular (and physical) radius of
the secondary is $\approx 72\%$ of the primary's radius.
In addition, the temperature of the third star is somewhat
hotter
than the secondary (e.g.\ $T_3=4700-5400$ K vs.\ $T_2=4600$ K).
If the third star was bound to the eclipsing binary, its
physical radius would be only $\approx 50/72=69\%$ the radius of
the secondary star.  Given that small size, it does not
seem likely the third star would be able to produce the same
{\em flux} as the secondary star if both stars are on the main
sequence.  On the other hand, if the third star were more
distant than the binary, then it could be more luminous than the
secondary (as its hotter temperature suggests it should be) but
at the same time have roughly the same flux. Thus
the fact that
the third star has a radial velocity similar to that of the
binary may be a coincidence.

Since ELC uses model-atmosphere
specific intensities, the overall third light level should be
reasonably well constrained given the wide bandpass coverage
of the available light curves.  Also, wide ranges for
the third light parameters were searched, and the solutions
converged on a situation where the third light contamination is
far from zero.
Thus we believe the radii we derive
for the primary and secondary should not be biased.

\section{Comparison With Model Isochrones and Discussion}\label{results}

Figure \ref{fig:Isochrone} shows the positions of the component stars
in KIC 6131659 in a
mass-radius diagram.  The figure also shows three theoretical isochrones
from the Dartmouth Stellar Evolution Program \citep[DSEP,][]{Dotter_2008}
and the empirical relationship derived by
\citet{Bayless_Orosz_2006}.
As noted earlier, most of the low-mass stars
with well-measured masses and radii are above the isochrones,
meaning the stars are larger than expected, given their masses.
In contrast, both stars in KIC 6131659 are on the same isochrone,
where the one with an age of 3.5 Gyr, [Fe/H]$=-0.25$,
[$\alpha$/Fe]$=0$, and a helium fraction of
$Y=0.2537$ formally provides the best fit with $\chi^2=0.5287$.
The isochrone with an
age of
2.5 Gyr, [Fe/H]$=-0.5$,
[$\alpha$/Fe]$=0$, and a helium fraction of
$Y=0.2537$
has a nearly identical $\chi^2$ (0.5397).   The metallicities of the best-fitting
isochrones match very well the metallicity found from the TODCOR analysis
(Table \ref{specparm}).   Figure \ref{fig:Isochrone} also shows a mass-temperature
diagram.  Both the primary and secondary are reasonably close to the best-fitting
isochrone.

\citet{Torres_2007}
introduced a parameter $\beta$ which is the correction factor needed
to make the model predictions of the radius agree with the
measured radius.  These are $\beta_1=1.001\pm 0.003$ for the primary
and $\beta_2=0.992\pm 0.009$ for the secondary, respectively.
These are consistent with unity, meaning no correction is needed to make
the evolutionary models agree with the observations.

Note that
the secondary in KIC
6131659 and the primary in Kepler-16 have
roughly the same mass as the secondary in
RX J0239.1-1028, whereas the radii differ by $\approx 0.1\,R_{\odot}$
(the secondary in RX J2039.1-1028 is the bloated star).
At these low masses, neither age
differences nor changes in the metallicity will
account for the large radius discrepancy.
There is therefore at
least one other parameter which influences where a star resides in this
diagram.

With the recent discoveries of the long-period eclipsing binaries
LSPM J1112+7626 \citep{Irwin_2011}, Kepler-16 \citep{Doyle_2011}, and now
KIC 6131659, the observational picture regarding the radii of low-mass
stars is becoming more complex.  The stars in LSPM J1112+7626
are inflated by about 4\%, which indicates that a very
long orbital period by itself does not automatically result in agreement with
the evolutionary models.  \citet{Irwin_2011} also showed that
LSPM J1112+7626 has a 65 day out-of-eclipse modulation of about 2\% which
was attributed to star spot activity.  As we discussed earlier, KIC 6131659
has an out-of-eclipse modulation of $\lesssim0.2$\%,
which presumably translates to
a lower level of star spot activity.  The primary star in Kepler-16 fits
on the model isochrone in the mass-radius diagram, whereas the secondary
star does not.
There is an $\approx 1\%$
peak-to-peak modulation in the out-of-eclipse light curve of Kepler-16
with periodicity of about 35 days
\citep{Winn_2011}, where the primary star is presumed to be the source of the
modulation.
Given these
three long-period binaries,
one might further speculate that
there might be a threshold of stellar activity level past which
these stars become inflated.

\citet{Feiden_2011} have recently presented improved evolutionary models
which were applied to the three stars in the eclipsing triple system
KOI-126 \citep{Carter_2011}.  A model isochrone with
an age of 4.1 Gyr and a metallicity of
$[{\rm Fe/H}]=+0.15$ reproduced the observed radii
of the stars reasonably well, with formal relative errors between the model
predictions
and observations of $\le 0.3\%$.
\citet{Feiden_2011} attributed the success of their models to an improved
treatment of the equation of state.  On the other hand, those same
models cannot match the observed radii components
of the well-known low-mass
binary CM Draconis, even when generous uncertainties in the metallicity
are considered.  Although the discovery of Kepler-16 was not announced
when the paper by \citet{Feiden_2011} was accepted for publication, it can be seen
from their Figure 2 that the secondary in Kepler-16 would lie
slightly above the model isochrones in the mass-radius diagram.
This seems to indicate a real dispersion in the observed
mass-radius relation for these fully convective stars.

\section{Summary and Thoughts on Future Work}\label{sec:Conclusion}

We have analyzed six Quarters of {\em Kepler}
data along with supporting ground-based photometric and
spectroscopic data and obtained precise and
accurate values for the masses and radii for
both stars in the long-period eclipsing binary
KIC 6131659.  The component stars in this binary
are not bloated, in contrast to nearly all other systems.
This suggests that at least one  parameter
in addition to the mass, age, and metallicity strongly
influences the ultimate radius of the star.

More observational work will be needed to better understand
the mass-radius relation for low-mass stars.  The radii of the
components in
KIC 6131659 agree with the model predictions for a 3.5 Gyr isochrone.
We have shown
that the present level of stellar activity in KIC 6131659 is
relatively low, which seems to suggest that high levels of spot
activity may contribute to the inflated radii found in
the short-period low-mass binaries.  On the other hand,
Kepler-16 has a somewhat higher level of stellar activity, and its
primary star also does not appear to be inflated.  We speculate that perhaps
there is a threshold level of activity past which the stars start to
become inflated.

Although the amplitude of any out-of-eclipse modulations
may not be a perfect indicator
of stellar activity, it is readily observable, especially in
{\em Kepler } data.
Are there binaries with very low
levels of out-of-eclipse modulations that nevertheless have stars with
inflated radii?  Similarly, are there additional binaries like
Kepler-16 with spot activity that have at least one star that
is not inflated?    Ground-based follow-up observations of these
binaries, especially the long period systems, can be challenging,
however, a sample of a dozen systems could lead to a
clearer understanding
of the mass-radius relation for low-mass stars.

\acknowledgments
We are grateful for the support from the National Science Foundation
via grants AST-0808145, AST-0850564, and AST-0908642,
from the {\em Kepler} Participating Scientist
Program via NASA grant NNX 08AR14G and the from
the {\em Kepler} Guest
Observer program via NASA grant NNX 11AC73G.
Kepler was selected as the 10th mission of the Discovery Program. Funding
for this mission is provided by NASA, Science Mission Directorate.
The Hobby-Eberly Telescope (HET) is a joint project of the University
of Texas at Austin, the Pennsylvania State University, Stanford
University, Ludwig-Maximilians-Universit\"at M\"unchen, and
Georg-August-Universit\"at G\"ottingen. The HET is named in honor of its
principal benefactors, William P. Hobby and Robert E. Eberly.

redpajama_set_name: RedPajamaArXiv


Manchester United manager Jose Mourinho has been relieved off his position with immediate effect today, December 18.
The Portuguese has left Manchester United after the club's 3-1 defeat to nemesis Liverpool in the English Premier League at Anfield.
The club statement reads "Manchester United announces that manager Jose Mourinho has left the club with immediate effect."
In two full seasons at Old Trafford, Mourinho won the Europa League and League Cup (2016-17) before finishing second in the Premier League last season and reaching the FA Cup final.
In that period since replacing Louis van Gaal, United's spending stands at £364.3m on eight buys.


text:
Blonde Redhead + I'm From Barcelona at McCarren Pool
Post Author: Nate Dorr
This week's installment of the McCarren Pool Parties proved to be a lesson in contrasts: the expansive, windswept rock currently occupying Blonde Redhead, preceded by the Bacchanalian indie-pop revelries of I'm From Barcelona. While the two are hardly comparable (though by the murmurs, those attending the pool for either one or the other alone tried anyway), it seemed that their pairing could be taken as either compliment or contradiction.
Blonde Redhead, having shed the remnants of their early no-wave inflections and propensity for noise with the sleek sorrow of 2004's Misery Is a Butterfly, continued their new-found polish with the release of 23 this year. The new songs, which formed the bulk of Sunday's set, had, even live, a certain pristine clarity, recreated faithfully and with every sound in place with the help of backing tracks. Pinned to their pre-existing song structures, Kazu Makino and the twins didn't really have many surprises in store for familiar audiences, and after the ridiculous number of people involved in the I'm From Barcelona set (the band has 29 members, I counted at least 23 present), the choice to play as a three piece with machine accompaniment gave them a sense of austere minimalism. At the same time, the band managed to couple that visual minimalism with constant poise, moving in measured, graceful gestures. Makino even managed to look composed and stylish during the few moments she let loose and danced, hair blowing across her face, to the music. So while their performance was somewhat less than kinetic, it left me hoping that I'll still look half as good as they did up there 15 or so years from now.
Openers I'm From Barcelona, by contrast, immediately eschewed such restraint in a blast of confetti cannons. I mean that entirely literally.
The 20-something-piece line-up (I doubt even they could keep track of everyone on stage), leaped, shouted and filled the air with exuberant pop choruses. I admit that I'm From Barcelona (incidentally from Sweden) weren't exactly on my musical radar before the show, but it was hard not to get caught up in the overall mood once things got moving (by the end, they managed to have most of the crowd waving their hands in time). Extra ridiculous party points for 1) covering "Like a Prayer" and 2) ending the set with a massive group bow accompanied by a pre-recorded 8-bit chiptune cover of their theme song 3) having a theme song.
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redpajama_set_name: RedPajamaCommonCrawl


Built in 1987, 5 Olive Drive Condo is a 32 unit condominium located in Hialeah, Florida. This community has 2 condo units for sale starting at $175,000. If you are interested in buying or renting a unit, click the "Condos for Sale and Rent" tab to see what is currently available, or click here to contact an approved realtor.
I would like more information on units at 5 Olive Drive Condo.


Pictured here with Doris (seated right) are sister Elaine Tyus (left) and (standing) daughters Mary Jane Syemore and Norma Dillon.
Doris Irwin of Marianna celebrated her 100th birthday on Saturday, January 26. A reception was held in her honor at the First Presbyterian Church in Marianna on Sunday, January 27. Many long time friends and family members were present to help celebrate the momentous occasion.


Elegant photo 50th wedding anniversary candy bar wrappers! Impress your guests or decorate your tables with these beautiful candy wrappers. Decadent cream and gold floral designs, with the couple's photo (then or now!), personalized with your information, Name & Wedding date on the front; the party date and custom thank you message on the back. These are great favors for 50th wedding vow renewals for the guests to take home.
Foil inner wrapper is a display/suggestion and is not included.


I've often wanted to print just the "selected text" in a message, but nothing seems to be available in Poco. Here's a tiny script that gets about 80% of the way there.
This may actually work due to a "bug" (or at least an undocumented feature) in PocoScript -- I do not recall ever seeing this documented. The script works because ReadBody, at least in versions 3 and 3.1 of Poco, will return the selected portion of the body if any selection has been made, and returns the entire body if no selection is made.
Obviously, you can insert your favorite word processor or print routine. And if you have a program that will print with a command line parameter, you could automate the whole thing. (I do not believe that Word has a documented switch to do this.) In addition, I've hard-coded the file location and names -- a more advanced version might be more flexible. This is just a proof of concept.
frazmi wrote: This may actually work due to a "bug" (or at least an undocumented feature) in PocoScript -- I do not recall ever seeing this documented.
I've also encountered this behavior in the past and I don't like it because I think that it's too dangerous. That is, if a person uses any PocoScripts, then the SaveMessage command will only save the selected text of the message (instead of the entire message) and it's unlikely that a user would notice this until it's too late.
What would you say to a new optional argument to ReadBody called "&AlwaysGetEntireBody"? If TRUE, the function would ignore the selection (if any) and return the entire message body. If FALSE, the function would work as it does now.
For true backward compatibility, it should default to FALSE, but could be set to TRUE to prevent the problem you mention.
frazmi wrote: What would you say to a new optional argument to ReadBody called "&AlwaysGetEntireBody"? If TRUE, the function would ignore the selection (if any) and return the entire message body. If FALSE, the function would work as it does now.
The behaviour of passing only the selected portion of the text is one that I have used in a number of scripts. I'm not sure what the best solution is, Pete has a valid point regarding possible problems with the current implementation but I know of a few scripts that will stop working as advertised should this behaviour be changed.
Well, guys, I would like all of the PocoScript commands (including the ReadBody/ReadRawBody commands) to work with the entire message by default. This is intuitive. I believe that the current behavior that happens after a user has selected text in the Preview Pane is unexpected, unintuitive, undocumented, and un-user-friendly.
We also have to consider the PocoMail users who will never write a PocoScript themselves but who use other people's scripts such as those in the Extras section of the website. Those people should never have to worry about whether or not they've selected text in the Preview Pane before they run our PocoScripts. It will never occur to them that PocoScripts work differently depending on whether or not they have selected some text in the Preview Pane.
I think that the behavior is dangerous even for experienced PocoScripters. It's too easy to click a toolbar button that runs a script without realizing that I've previously selected some text in the Preview Pane. It's also possible that the selected text in the Preview Pane is not currently visible because that part of the message has been scrolled out of sight with the scrollbar.
I think that Michael and I agree in general and I think that we both want what's best for both expert and novice users of PocoMail. My opinion possibly differs from his because I think that the %message variable should always work with the entire message and that people who have been using the undocumented behavior should be asked to do a search-and-replace on their scripts and change all occurrences of the %message variable (where they use the undocumented behavior) to a new one such as %selectedTextMessage. I don't think that it's fair to ask the majority of PocoScript programmers to change our scripts just because some people are using the undocumented behavior.
Michael, I wonder how many changes would be required for people who are using the current behavior. It seems to me that the current behavior would only be useful in a small number of situations and that it would be relatively easy for them to change their scripts to handle these special situations. What do you think?
I don't think that it's fair to ask the majority of PocoScript programmers to change our scripts just because some people are using the undocumented behavior.
As far as I can tell, nobody so far has suggested this. If the existing readbody function were modified as I suggested (by adding a new optional parameter), every script currently in existence would continue to function exactly as it does now. Thus, if the [bug | undocumented behavior | whatever] currently causes a problem if there's selected text in the preview pane, it would continue to cause problems.
Having said that, I also like the idea of a new variable construct, %SelectedTextMessage. I don't know which would be more difficult to implement, nor which might have more side effects, but I would be satisfied with either solution.
Pete wrote: Well, guys, I would like all of the PocoScript commands (including the ReadBody/ReadRawBody commands) to work with the entire message by default. This is intuitive. I believe that the current behavior that happens after a user has selected text in the Preview Pane is unexpected, unintuitive, undocumented, and un-user-friendly.
A quick scan of my scripts reveals I have 10-12 that rely on the selected text being passed to the %Message variable. I have not done a scan of the scripts in the extras area to see which ones use this feature.
I have, in the past, asked Slaven to create a %FullMessage system variable because there have been times when I'd like to know whether or not the user has selected a portion of the message.
The problem, as I see it, is that changing current behaviour may not be ideal. There may be people out there who have scripts installed on their system that are using this feature. If the ReadBody command were to change then their scripts would stop working as desired and they wouldn't necessarily know why. It could cause problems for them (suppose their business relied on this feature for some purpose).
I just ran into a problem with filing a message -- I couldn't figure out why I couldn't find this message I was sure I had received, and it turns out that when I used a button script to file it to a saved folder, I must have had some text selected, as part of the message is there.
Is there any way to move a message from one folder to another without only copying the selected text? I've looked everywhere and can't find anything -- seems like such a trivial need that I must just be missing it.
Now, obviously I can right click a message and use the "Move to Folder" submenu, but I've got a couple buttons that I use to run a script -- for commonly used folders that I file stuff to.
Not while using a script, see my alternate method in this thread.
My alternate solution was posted at Wed Jun 28, 2006 5:21 pm. It suggests using manual filter groups. To the best of my knowledge you cannot assign these to a button but you can use keyboard shortcuts to execute them.
ok -- I'm stupid -- first off I didn't notice that "This Thread" was a link -- and I somehow didn't realize there was a reply to my question in the other thread. Thanks for the info -- still hoping they'll make a %fullmessage available, or buttonable filters.


Butterscotch Palkova, today we will see how to prepare milk halwa / thirattipal with butterscotch at home with step by step photos. Butterscotch Palkova is made using packet milk, butterscotch chips and sugar. For a bit of extra flavor, try adding a pinch of cardamom powder.
This is a very simple recipe but need time to prepare. I have never tried quick version of preparing palkova using microwave. To prepare butterscotch palkova, heat 1 liter packet milk. You can also try with 500 ml milk but the final quantity will be very less. Using 1 liter milk, you can serve palkova to 2 people. Once milk starts boiling, keep the flame to low and let it cook till the quantity of milk reduces and reaches thick consistency. At this stage you need to add butterscotch chips and sugar.
I have added very less sugar since butterscotch also has sweetness. Crush the chips lightly and then use it. Milk halwa / Butterscotch palkova is very light. Instead of sugar, you can also try with jaggery. If using jaggery, then add it after removing palkova from the flame to avoid curdling. I have used aavin blue packet milk (toned milk). The same cooking procedure is followed to prepare mawa / plain khoya, where we dont add any sugar or jaggery.
Some of the other milk based sweet recipes shared in my blog, Simple Palkova, Apple Peda, Easy Paneer Mawa Barfi, Chocolate Milk Powder Peda and Khoya Gulab Jamun. If you try any of my recipes, then do share your feedback with us.
Heat milk in a pan or kadai. I have used stainless steel vessel to heat milk. Switch the flame to low and let it boil. Depending on the vessel you use, the cooking time may vary. Once milk starts boiling, stir it with a spoon or flat ladle and scrape the sides of the vessel.
Stir it every 5 or 10 minutes and scrape the sides. Milk level will start reducing and the color will also change. Keep on stirring for every ten minutes. When the mixture looks thick with some liquid left, add butterscotch and sugar. Keep stirring now. You need to keep stirring to avoid sticking at the bottom. When all the liquid is absorbed and you get thick halwa like mixture, switch off the flame. Add a pinch of cardamom powder and garnish with chopped pistachio. Serve hot or at room temperature.
Nandri Sowmya 🙂 I liked it more compared to the one we make with sugar..


text:
Responding to the heartbreaking events in Afghanistan
RCPsych President, Dr Adrian James responds to the situation unfolding in Afghanistan and the implications for veterans' mental health.
The dramatic events unfolding in Afghanistan have been heartbreaking. It has been uncomfortable and upsetting to watch thousands of people fleeing their homeland in pursuit of safety. The threat to women and girls, and other marginalised groups is particularly troubling. Our thoughts go out to the people of Afghanistan and we hope that a peaceful solution is found quickly.
Many will seek asylum in the UK and will no doubt need mental health support because of what they've endured and the journeys they'll be undertaking. The College will be working to improve conditions for asylum seekers and also the mental health support available to them. We are also calling on the government to scrap its Nationality and Borders Bill, which will exacerbate the mental health problems of asylum seekers.
Roughly 150,000 veterans in the UK have been deployed in support of the Afghan conflict. They may be left questioning the meaning of their service or whether it was worth the sacrifices they and the Afghan people made. As a result, some may be feeling distressed, especially those with pre-existing mental health problems, and may need to access professional care.
Some of our psychiatrists will be veterans and many of us will have veterans under our care. We need to ask them how they're feeling, listen to them with empathy, and provide them with any additional support they might need. It's vitally important for them to know that they've done their duty and that they are in no way responsible for the outcome and the tragedy that is unfolding.
The Royal College of Psychiatrists' Centre for Quality Improvement has launched a national network for veteran mental health services and is introducing new, specific quality standards for these organisations. This work to improve these services is now even more needed than it already was and will help improve outcomes for veterans by improving the quality of service provision and by providing consistency across services. If you work in a specialist service providing mental health support to veterans and want to be involved in this important work then do get in touch with the College.
Dr Adrian James
Adrian was elected President in 2020. He holds this role until 2023 and leads the RCPsych on behalf of its members and associates.


text:
EDWARD WITHAM JR. GRADUATED 1998 INDUCTED 2004
EDWARD WITHAM JR. AHS Class of 1998
Witham was a three-year letter winner in both football and baseball at Alliance and earned All-Federal League honors in both sports. He was first-team All-Ohio in baseball his junior and senior year at AHS. In football, he played outside linebacker for the Aviators while earning all-league honors.
Ed is a graduate of Wright State University, in Dayton, Ohio, where he majored in elementary education, graduating Summa Cum Laude with a 3.95 GPA. He served as a teaching assistant for the Physics Department at Wright State in 2001.
He was a graduate assistant for the Education Administration, Research and Foundations Office at Youngstown State University from 2003-2004 and earned his Administrative certificate in 2004.
 Ed is the first-ever head football coach at Youngstown Christian School which began its football program in the fall of 2004, a former football coach at Alliance and Marlington High School and served as a football coach at Baker Junior High and Green High School.
He and his wife, Kim, and daughter, Leah, reside in Alliance.


text:
Practice Part 1
Business, Finances, General, Marketing, Social Media
Multiple Income Streams Soothe Therapist's Financial Anxiety (part 1)
Relying solely on direct clinical hours may leave private practitioners financially vulnerable to income instability. Since client hours in private practice can vary greatly depending on the time of year, state of the economy, number of new referrals, and several other factors, developing multiple income streams can help you to create a more stable income. "By having the other income streams in place, I have been able to be less susceptible to the ebbs and flows that occur in private practice during difficult economic times," says The Rev. Christopher L. Smith, LCAC, LMHC, LMFT. In addition to providing income stability, diversifying your professional activities with multiple income streams allows therapists to explore a variety of interests, to express creativity, and to get paid for their passions.
In addition to clinical hours, I own and serve as clinical director of a private therapy clinic where I oversee and supervise 10 therapists, write for PsychCentral and other publications, work as a relationship and emotional health media contributor, do public speaking, provide consultation to therapists building a private practice, and I'm currently writing my first book. Curious about what other private practitioners are doing to add to income stability I reached out to several successful colleagues to see what additional income streams they've developed. Here's a sampling of what other therapists are doing to diversify their professional life and achieve greater income stability.
Write and publish a book
Many therapists have taken their clinical expertise and turned it into a book. For example, Frank J. Sileo, PhD has written three children's books, including Bug Bites and Campfires: A Story for Kids about Homesickness (Health Press, 2009). Clinical Psychologist Dr. John Duffy took his passion for parenting and authored a book The Available Parent: Radical Optimism For Raising Teens and Tweens (Viva Editions, 2011). What areas of expertise could you write about?
Write for print publications
Supplementing clinical work, Terrie Browning, LPC, CFC, DCC writes for a column "My Healthy Mind" for a local magazine My Metro You. Not only does it provide additional revenue but she says it's also personally fulfilling. Of writing for publications she says, "Writing allows me to share knowledge on topics that are a concern for many people and offers a way for me to network myself." Therapist Karen R. Koenig, LCSW, M.Ed. has successfully written for professional publications including Social Work Focus, Social Work Today, Addiction Treatment Forum, and The Newsletter for the Society for Family Therapy and Research, adding an additional income stream.
Create a therapeutic product
Have you considered creating and selling a product based on your clinical expertise? Stephanie Ann Adams, M.A., LPC of Beginnings Counseling & Consulting, created a hybrid counseling/video series for premarital counseling through Twogether in Texas. To help families deal with the stress of relocation Jill Kristal, President of Transitional Learning Curves, developed a game and book series called 'Our Move'.
Develop a professional online network
The internet allows for many options for therapists to create passive income through membership sites. In addition to writing a local magazine column and providing clinical work, Browning, with the help of her adult children, developed a professional wellness center online called Experts Now. This online center offers wellness experts an avenue to offer services and sell products for a commission creating additional income for Browning.
Contract as a consultant
Consider asking yourself, "Which companies or organizations may want to tap into your areas of expertise?" Therapist Dr. Mario Kirk, LPC, Director, A Blessed Child, LLC, performs psychological testing for local attorneys and schools. Women's reproductive health specialist Pec Indman EdD, MFT consults and trains for county health programs and for the US Federal government.
Are you developing multiple streams of income to supplement your direct care hours? Please share your ideas in a comment below.
Watch for multiple income streams part 2 later this week!
Tagged: Bug Bites, Cfc, Children S Books, Clinical Director, Clinical Expertise, Clinical Psychologist, Conflict Resolution, Contract Work, Ebb And Flow, Economic Instability, Economic Stability, Economic Times, Economic Uncertainty, Emotional Health, Health Media, Health Press, Homesickness, Income Insecurity, Income Sources, Income Stability, John Duffy, Julie Hanks LCSW, Kristal, Lcac, Lcsw, Learning Curves, Licensing Fee, Lmft, Lmhc, Lpc, Marriage Education, Marriage License, Move Series, Multiple Income Streams, Passions, Personal Benefit, Physical Location, Practice Part 1, Premarital Counseling, Private Practice, private practice toolbox, Private Practitioners, Private Therapy, private therapy practice, Professional Activities, Radical Optimism, Relocation Issues, S Books, Sileo, Stable Income, Stephanie Ann, Streams Of Income, Successful Women, Twogether, Wellness Center


Add a touch of Parisian chic to your desk with this chambray stripe journal. It's lined pages are perfect for recording ideas and dreams. And the double grosgrain ribbons will help you keep your place. The carefully sourced premium chambray fabric truly reflects the style of Sugar Paper. Personalize it by adding your monogram in gold foil.


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Q: In Kafka, How can we get the metadata of a topic? In Kafka, How can we get the metadata of a topic? If there is an option to get metadata and if I'm trying to get the metadata of a topic that doesn't existing, what happens?

A: kafka-topics --describe --bootstrap-server localhost:9092 --topic name
Or refer Javadoc for AdminClient class, or similar for a programming language of your choice

redpajama_set_name: RedPajamaStackExchange


Location! Location! Prime downtown london! Three level commercial & residential great for business owner or investment! Main floor runs successful convenience store " Richmond Magazine and Variety' over 20 years. Three bedrooms unit on the second and third floor that were newly renovated in 2004. Newer shingle 2013. Running business, collecting rent. Excellent opportunity! Currently the owner runs the business and live in one unit. Potential NOI $51,200 if all rented out. Please call the listing for detail!


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Q: Can't use LINQ in EF Where expression for lambda property I changed the LINQ expression like this.
public async Task<IEnumerable<Thing>> Get(bool all)
{
  List<Thing> output = await Context.Things
    //.Where(_ => all || _.DeletedOn == null && _.Deletedon < DateTime.Now)
    .Where(_ => all || _.Active)
    .ToListAsync();
  return output;
}

Apparently, it caused the following error.

InvalidOperationException: The LINQ expression 'DbSet .Where(l => False || l.Active)' could not be translated. Either rewrite the query in a form that can be translated, or switch to client evaluation explicitly by inserting a call to either AsEnumerable(), AsAsyncEnumerable(), ToList(), or ToListAsync().

Well, I do have a call to AsListAsync() and I'm a bit buffeled that such a simple conditional wasn't interpretable by .NET Core EF. I suspect I might be missing something else.
The class Thing looks like this.
class Thing
{
  ...
  public DateTime? DeletedOn { get; set; }
  public Active => DeletedOn == null && DeletedOn < DateTime.Now.
}

Checking the provided link gave me nothing.

A: As others have mentioned, the expression bodied member getter is actually regarded a method call, which can't be parsed by a Linq QueryProvider into native SQL, so you'll need to again undo your 'DRY' code and instead expand the predicate logic in the Active property directly into your Linq Query, or alternately you would need to pass the entire Expression Tree or IQueryable to a method like Active so that it could compose the predicate into it (which seems overkill).
Also, as per comments, there's a logical issue - _.DeletedOn == null && _.Deletedon < DateTime.Now will return false, meaning the query is then all or nothing based on the value of the all parameter. At a guess, you're looking for a conditionally applied 'logical delete' filter, which also allows for future dated deletion, i.e. any record which hasn't yet been deleted is to be regarded as active, or any record which has a null deletion date hasn't been deleted at all.
And finally, for most RDBMS, especially SQL Server, it is usually not a good idea to add a hard coded predicate (like all) into a WHERE filter, as this can mess with the query plan caching. In your case, the all flag filtering logic simply decides whether you want to include logically Deleted data or not. IMO, I would instead conditionally compose the query like follows to avoid doing unnecessary filtering in SQL.
Putting this all together, the query would be:
var query = Context.Things;
if (!all)
{
   query = query.Where(t => t.DeletedOn == null || t.Deletedon > DateTime.Now)
}
var output = await query
   .ToListAsync();
return output;

A: See breaking changes in .Net core 3.0
One solution (though not advised) could be the following:

If a query can't be fully translated, then either rewrite the query in a form that can be translated, or use AsEnumerable(), ToList(), or similar to explicitly bring data back to the client where it can then be further processed using LINQ-to-Objects.

So as it would happen before, get the dbset with a translatable query and filter later on with whatever C# linq to Objects magic you'd like.
Without having tested it, I believe that EF can't translate your Expression bodied member. Did it work when you tried with the following?
   .Where(_ => all || _.DeletedOn == null && _.Deletedon < DateTime.Now)

A: The problem is in the expression body in the public field Active.
EF could not translate this expression Active => DeletedOn == null && DeletedOn < DateTime.Now.

A: Try inserting a call to either AsEnumerable(), AsAsyncEnumerable(), ToList(), or ToListAsync() before filtering the records i.e. in this case before Where condition.