text:
\section{Introduction}
\label{introduction}

The importance of eclipsing binaries for advancing our understanding of stellar structure and evolution
was reviewed by \cite{2012ocpd.conf...51S}. Eccentric eclipsing binaries contribute particular
insights in this respect \citep[see, e.g.,][]{2019A&A...628A..29C}. For eccentric systems,
high-precision photometry from TESS \citep{2015JATIS...1a4003R} enables tests of relativistic
predictions of apsidal motion to be performed with unprecedented accuracy \citep{2021A&A...649A..64B}.
A recent study \citep{2018ApJS..235...41K} implied a possible relation between the orbital period and
the apsidal motion period among known systems displaying apsidal motion; however, the possibility of
observational bias in this respect has not been discounted. Notwithstanding this caveat, the existence
of a hard upper limit to the eccentricity (which is a function of the orbital period) has been firmly
established in the observed period-eccentricity ($P-e$) diagram. The appearance of the observational
$P-e$ diagram corresponds to theoretical expectations based on the dynamics of the tidal
circularization process; however, tidal effects are expected to have diverse impacts on early- and
late-type stars because of their differing internal structures. A corresponding
divergence between the  behavior of eclipsing systems composed of hot stars and systems composed of
cool stars was demonstrated recently \citep{2016ApJ...824...15V}. These statements call for an
expansion of the number of eccentric systems for which physical parameters can be obtained with high
precision, so that theoretical models may be assessed more incisively. In this study, we present a
study of two previously unexplored eclipsing eccentric systems, using both photometry and spectroscopy.

\section{Sources of data}

The data for TYC 5378-1590-1 and TYC 8378-252-1 were obtained partly from dedicated observational
campaigns on these stars. This is specifically true of the spectroscopic data, where several dozen
radial velocity observations were obtained during multi-year campaigns using the Cassegrain-mounted
spectrograph on the 1.9m telescope at the South African Astronomical Observatory (SAAO).

\subsection{Spectroscopy}
\label{spectroscopy}

\begin{figure*}
  \centering
    \includegraphics[scale=2.3]{tyc5378_spectra.pdf} \\
    \includegraphics[scale=2.3]{tyc8378_spectra.pdf}
\caption{Sample spectra for TYC 5378-1590-1 (upper diagram, for phase 0.56) and TYC 8378-252-1 (lower
diagram, for phase 0.01) obtained in this study. While the hydrogen Balmer lines and the Mg II (4481)
line are indicated in the spectrum of TYC 5378-1590-1, many metallic lines are also indicated in the
spectrum of TYC 8378-252-1. } \label{sample_spectra}
\end{figure*}

Spectroscopic observations of TYC 5378-1590-1 and TYC 8378-252-1 were conducted with the Spectrograph Upgrade: Newly Improved Cassegrain (SpUpNIC) instrument \citep[see][for
details]{Crause_etal_2016,Crause_etal_2019}  mounted at the Cassegrain focus of the 1.9m telescope at
the SAAO.

We selected grating 4 of the spectrograph. This 1200 lines/mm grating has a wavelength coverage of 400
-- 525 nm with a blaze peak at 510 nm and a resolution of 0.062 nm/px (corresponding to a resolution of
approximately 80 km s$^{-1}$ in radial velocity and an approximate resolving power $R = 3000$ at the
wavelength of the H$\beta$ line).  The wavelength range between 400 and 525 nm provided a spectral
interval that allowed an accurate derivation of radial velocities (RVs) of both components on most of
the spectra obtained. We used a slit width of 1.35 arcsec for all spectroscopic observations of the two
eclipsing systems and the associated RV standards, which were observed contemporaneously. A total of 62
and 86 spectra were obtained for TYC 5378-1590-1 and TYC 8378-252-1, respectively, across the 2019,
2020, and 2021 observing seasons.

HR 3383 (A1V, $V_r = 2.80$ km ${\rm s}^{-1}$) and HR 6031 (A1V, $V_r = -5.10$ km ${\rm s}^{-1}$) were
observed contemporaneously as standard stars for the RV measurements of the two binary systems. The
exposure times were set at the maximum feasible value of 1200 seconds for each spectrum because of the
faintness of the two targets (exposure times longer than 1200 s are usually compromised by a high
frequency of cosmic ray events in the spectra at the SAAO site). The relatively large errors in the
measured RV values (see Figs. \ref{FigRV_TYC5378} and \ref{FigRV_TYC8378}) are predominantly the result
of this upper limit on the feasible exposure time for these two relatively faint targets. Arc spectra
using a Cu-Ar lamp were taken as comparison spectra before and after each stellar spectrum. A set of
quartz-iodine lamp images was also taken every night for flat-field calibrations. Standard IRAF
procedures were used for the spectral data reduction and calibrations.

An example of the observed spectra for each of TYC 5378-1590-1 and TYC 8378-252-1 is shown in Fig.
\ref{sample_spectra}. The sample spectra in Fig. \ref{sample_spectra} were selected from the
conjunction phases of the components, with the more massive component transiting in front of the less
massive component in each instance. The characteristic lines of early A-type stars are seen in the
spectrum of TYC 5378-1590-1, whereas the characteristic lines of middle F-type stars are seen in the
spectrum of TYC 8378-252-1.

\subsection{Radial velocities}
\label{RVs}

The cross-correlation method was applied to derive RVs of the component stars of these two eccentric
binaries, using the IRAF package {\sc Fxcor} \citep{Tonry_Davis_1979,Popper_Jeong_1994}. The spectral
region around the Mg II (4481) line, which is the most prominent line apart from the hydrogen Balmer
lines (see Fig. \ref{sample_spectra}), was used for the RV calculations of TYC 5378-1590-1 (with
spectral type A0V). For TYC 8378-252-2 (with spectral type F4/5V), the spectral range from 4360 to 4800
{\AA} containing Mg II (4384, 4481, and 4668) and Fe I (4383) lines was used for the RV calculations.
The spectra of HR 6031 and HR 3383 were used as a template for deriving the  RVs of the binary components.
The calculated RVs obtained from the cross-correlation method are depicted in Figs. \ref{FigRV_TYC5378}
and \ref{FigRV_TYC8378}  and are listed in Tables~\ref{tableA1} and \ref{tableA2} in Appendix \ref{secA}
for TYC 5378-1590-1 and TYC 8378-252-1, respectively.

\subsection{Photometry}
\label{photometry}

Our spectroscopic data were obtained from our own long-term observing campaigns; instead, we drew the
photometric data primarily from open surveys, satellite missions, and other long-term databases. We
relied primarily on TESS satellite data \citep{2015JATIS...1a4003R} for TYC 5378-1590-1. We used the
{\tt{lightkurve}} package \citep{2018ascl.soft12013L}  to extract the photometry from the TESS
database. For TYC 8378-252-1, we based our light curve solution exclusively on ground-based ASAS-SN data
\citep{2014ApJ...788...48S, 2017PASP..129j4502K}.

The primary databases mentioned above were supplemented with older data from the CRTS
\citep{2017MNRAS.469.3688D}, NSVS \citep{2004AJ....127.2436W}, and ASAS \citep{2002AcA....52..397P}, as
well as the discovery data for TYC 5378-1590-1 \citep{2013IBVS.6100...12M}, as inputs for our analysis.

\section{Analysis}
\label{analysis}

In view of the large TESS pixels (especially problematic in dense stellar fields with many neighboring
stars appearing on a pixel together with the target star), coupled with artificial instrumental trends
in the TESS photometry, a flattening method has to be applied to TESS data, and great caution needs to
be exercised when interpreting these data and conducting consequent  modeling. However, the TESS light
curves constitute the best available photometric data for this system by a long margin.

The {\sc PHOEBE package}, version 0.32svn \citep{2005ApJ...628..426P}, which was originally based on the
Wilson-Devinney code \citep{1971ApJ...166..605W} and applies Roche geometry, was used for our analysis
of the photometric data. By virtue of the good phase coverage of both the photometric and radial
velocity data for both our systems, our modeling procedure generated realistic physical parameters for
both of the eclipsing components in each system, and for their mutual orbits. Only a few additional
assumptions were required. The principal assumptions related to the gravity-brightening coefficients
and the albedos for both stars, together with the assumption of a pseudo-synchronization of rotation in
periastron for both systems; the obtained spectra were too noisy to be used for deriving the actual
rotational velocities of the components.

 \begin{figure}
   \centering
   \includegraphics[width=0.49\textwidth]{LC_OK_TYC5378.png}
   \caption{Light curve of TYC 5378-1590-1 based on TESS data and the solution provided with PHOEBE. The black crosses are TESS data and the red line is the PHOEBE solution.}
   \label{FigLC_TYC5378}
  \end{figure}

  \begin{figure}
   \centering
   \includegraphics[width=0.49\textwidth]{RV_TYC5378.png}
   \caption{Radial velocity curves of TYC 5378-1590-1. The red curve applies to the primary component; the black curve applies to the secondary component.}
   \label{FigRV_TYC5378}
  \end{figure}

  \begin{figure}
   \centering
   \includegraphics[width=0.49\textwidth]{TYC5378.png}
   \caption{O-C diagram for the system TYC 5378-1590-1. The black symbols and     curve denote the primary component; the blue symbols and   curve denote the secondary component. A slow change in the omega angle is only barely noticeable.}
   \label{OCdiagrTYC5378}
  \end{figure}

    \begin{figure}
   \centering
   \includegraphics[width=0.49\textwidth]{TYC5378_Residuals.png}
   \caption{O-C diagram of residuals for the system TYC 5378-1590-1 after subtracting the apsidal motion fit.}
   \label{OCdiagrTYC5378resid}
  \end{figure}

\begin{table}
  \caption{Parameters obtained from the LC+RV fitting of TYC 5378-1590-1 and TYC 8378-252-1.}
  \label{LCRVparam}
  \centering
  \small
\begin{tabular}{lcc}
\hline \hline \multicolumn{1}{l}{Parameter} & \multicolumn{1}{c}{TYC 5378-1590-1} &
\multicolumn{1}{c}{TYC 8378-252-1} \\
\hline \hline
$T_0$ (HJD) & 2453946.517       & 2451981.779 \\
$P$ (d)     & 3.7323493         & 2.8776874 \\
\hline
$A$ (R$_{\odot}$) & 15.88 $\pm$ 0.07& 11.39 $\pm$ 0.15 \\
$V\gamma$ (km/s) & 1.38 $\pm$ 0.45  & 46.8 $\pm$ 1.4 \\
$e$         & 0.308 $\pm$ 0.037     & 0.193 $\pm$ 0.012 \\
$\omega$ (deg) & 18.0 $\pm$ 7.1     & 142.7 $\pm$ 8.3 \\
$q=M_2/M_1$ & 0.853 $\pm$ 0.008     & 1.14 $\pm$ 0.04 \\
$i$ (deg)   & 85.52 $\pm$ 0.06      & 87.08 $\pm$ 0.26 \\
$T_1$ (K)   & 9800 (fixed)          & 6308 $\pm$ 209 \\
$T_2$ (K)   & 8824 $\pm$ 87         & 6600 (fixed) \\
$\Omega_1$  & 9.344 $\pm$ 0.019     & 8.637 $\pm$ 0.036 \\
$\Omega_2$  & 9.549 $\pm$ 0.015     & 8.421 $\pm$ 0.062 \\
$r_1$ (mean)    & 0.16 $\pm$0.01    & 0.14 $\pm$0.01 \\
$r_2$ (mean)    & 0.22 $\pm$0.01    & 0.16 $\pm$0.01 \\
$L_1$ (TESS)    & 0.55 $\pm$0.02    & -- \\
$L_2$ (TESS)    & 0.33 $\pm$0.02    & -- \\
$L_3$ (TESS)    & 0.12 $\pm$0.05    & -- \\
$L_1$ (ASAS-SN g)   & --            & 0.43 $\pm$0.03 \\
$L_2$ (ASAS-SN g)   & --            & 0.57 $\pm$0.03  \\
$x_1$, $y_1$    & 0.78, 0.27        & 0.55, 0.22 \\
$x_2$, $y_2$    & 0.59, 0.29        & 1.18, 0.23 \\
\hline
\end{tabular}
\end{table}

\begin{table}
    \caption{Apsidal motion parameters of TYC 5378-1590-1 and TYC 8378-252-1.}
    \label{am_parameters}
  \centering
        \small
            \begin{tabular}{lcc}
            \hline \hline
            \multicolumn{1}{c}{Parameter} & \multicolumn{1}{c}{TYC 5378-1590-1} & \multicolumn{1}{c}{TYC 8378-252-1}  \\
            \hline \hline
$T_0$ (HJD)   & $2453946.517 \pm0.005$  & $2451981.779 \pm0.016$ \\
$P$ (d)       & $3.7323493 \pm0.0000468$    & $2.8776874 \pm0.0000101$ \\
$e$           & $0.308 \pm0.037$        & $0.193 \pm0.012$    \\
$\omega$ (deg)& $18 \pm7$           & $143 \pm8$ \\
$\dot{\omega}$  (deg yr$^{-1}$) & $0.036 \pm0.011$  & $0.362 \pm0.108$ \\
$U$ (yr)    & 10000 $\pm3056$           & $995 \pm297$ \\
            \hline
            \end{tabular}
\end{table}

\subsection{TYC 5378-1590-1}
\label{tyc5378}

TYC 5378-1590-1 (= 2MASS J06454395-0850355 = TIC 120023539, RA 06$^h$ 45$^m$ 43.95$^s$ DE -08$^\circ$
50$^\prime$ 35.50$^{\prime\prime}$, V = 10.9~mag) is a known eccentric eclipsing system. However, its
properties were  derived  very approximately in previous studies. The system was first identified as
an eccentric eclipsing system with a correct orbital period by \cite{2013IBVS.6100...12M}.
The system was included in our previous study \citep{2018A&A...619A..85Z}, where we used the
  poor photometric data from the discovery paper and no spectroscopy. In that study a very slow
rate of apsidal motion and an eccentricity of 0.32 were derived for the system.

Our present study addresses this system with far superior TESS data and a longer time span of photometric observations, and with the recent spectroscopy obtained as part of our long-term campaigns from 2019 to  2021. The results of our fitting procedure are listed in Table \ref{LCRVparam} and plotted in Figs. \ref{FigLC_TYC5378} and \ref{FigRV_TYC5378}. The fit of the TESS data is superb. The RV data are much noisier (for the reasons mentioned earlier), but still present valuable information for inclusion in our analysis.

The solution presented in Table \ref{LCRVparam} was derived from our combined fit using both LC and RV
data together and constitutes a statistically meaningful result. A significant contribution of third
light emerged from the TESS data, in addition to the fluxes from the two main components. This effect
was caused by the relatively large TESS pixels, which allowed nearby stars unrelated to the TYC
5378-1590-1 system to contribute flux to the same pixels as the main target. We cannot speculate
about any third body in the system since no variation in the $O-C$ diagram is visible (see below).

Three different methods were used to determine the effective temperatures of the components of TYC
5378-1590-1, a system that has not been widely covered in  the literature (e.g., it had no assigned spectral
type prior to this study). First,  the color index of $B-V = 0.01 \pm0.09$, which was derived from the
\citet{Hog_etal_2000} study, shows that the spectral type of the system is close to A0. Second,  the
solution of the RV curves obtained in the present study corresponds to a mass of the primary component
of approximately 2 M$_{\odot}$, which is in agreement with a spectral type of A0. Third,  using the
line-matching method, especially for the H$\gamma$, H$\beta$, and Mg II 4481 lines in the observed
spectra of the components and the sample spectra of the early A-type main-sequence stars in the
\citet{Gray_Corbally_2008} book, the spectral type of the system was estimated to be close to A0.
Based on these results, we adopted a temperature of $9800 \pm200$ K, corresponding to a spectral type
of A0V in the calibrated data of \citet{Pecaut_Mamajek_2013}. The effective temperature of the primary component, which has a higher mass according to the solution for the RV curves, was taken as 9800 K, and this value was fixed in the WD iterations, whereas the effective temperature of the secondary component was adjusted during iterations.

As we   discuss in Section \ref{evolution}, both eclipsing components appear to be normal stars
located on the main sequence, most likely of spectral types A0 and A3. The primary
component might be slightly smaller in volume than  expected for a typical A0V star, while the
secondary appears slightly hotter than a typical A3V star. The locations of the two components on the
main sequence correspond with the young ages implied by the presence of an eccentric orbit.

Using all available photometric data for the star TYC 5378-1590-1, we also performed a period analysis
using the longest possible time interval. The data added to those used in our former study
\citep{2018A&A...619A..85Z} were primarily composed of the TESS observations, supplemented by more
recent ASAS-SN data. However, our results indicate only a slight evolution of the apsidal angle
$\omega$, meaning that the apsidal motion occurs at a very slow rate (on the order of thousands of
years). No additional trend is visible in the residuals, which are perfectly symmetric in their
distribution (see Fig. \ref{OCdiagrTYC5378resid}).

\subsection{TYC 8378-252-1}
\label{tyc8378}

TYC 8378-252-1 (= ASAS J185951-4711.8, RA 18$^h$ 59$^m$ 51.29$^s$ DE -47$^\circ$ 11$^\prime$
47.59$^{\prime\prime}$, V = 11.2~mag) has been mentioned only briefly as an eclipsing binary system in
prior work based on survey data from CRTS and ASAS. It was also included in our previous study
\citep{2018A&A...619A..85Z}, where we derived an eccentricity of $e=0.167$ for its orbit, and slow
apsidal motion with $U = 558$~yr. A more detailed analysis of this star has not been published to date.

The star was checked in various databases for photometric indices or any other indication of its color
or effective temperature. Markedly different values were obtained from various sources, for example,
$T_{eff}=6640$~K \citep{2017AJ....154..259S}, $6790 \pm 318$~ K \citep{2019AJ....158...93B}, and
$7004~$K \citep{2006ApJ...638.1004A}. Similar discrepant values were found for its distance. For
example, \cite{2006ApJ...638.1004A} presented the star's distance as 51~pc, whereas GAIA EDR3
\citep{2020yCat.1350....0G} presents a distance of 670~pc.

Therefore, three methods (as for the temperature determination of TYC 5378-1590-1) were applied to
determine the surface temperature of TYC 8378-252-1. First, according to the color index of $B-V = 0.60
\pm0.18$ derived from the study of \citet{Hog_etal_2000}, both  components are thought to be late
F-type main-sequence stars. Second,  the solution of the RV curves obtained in this study corresponds to a
mass of the more massive (secondary) component of approximately 1.3 M$_{\odot}$, which implies a
spectral type close to F5V. Third, using the line matching method for the H$\gamma$, H$\beta$, Ca I
(4226), Mg II (4481), Fe I (4383, 5041), Fe II (4923), and Mg I (5167 - 5183) triplet lines,  and using the
(CH) G band (see Fig. \ref {sample_spectra} for TYC 8378-252-1) in the spectra observed at the
conjunction phases of the secondary component and the sample spectra of the middle F-type main-sequence
stars in the book by \citet{Gray_Corbally_2008}, the spectral type of the secondary component was estimated
as F5V. Based on these results, we assigned a temperature corresponding to a spectral type of F5V,
equal to $6600 \pm200$ K, according to the calibrated data of \citet{Pecaut_Mamajek_2013}. The
preliminary solution of the ASAS-SN light curves indicated that the light contribution of the secondary
component is dominant. The secondary component also has a higher mass according to the solution of the
RV curves. Therefore, the temperature of the secondary component ($T_2$) was fixed at 6600 K, and the
temperature of the primary component ($T_1$) was adjusted in the iterations.

No TESS photometry for this system is yet available (TESS will observe the system in July 2023), and
the existing photometry is of low quality. However, we used the best available photometric data
obtained by the ASAS-SN survey in its $g$ filter for a photometric analysis. We fitted these data using
PHOEBE together with the radial velocities (29 primary and 46 secondary velocities), resulting in the
solution presented in Table \ref{LCRVparam}. The fits are plotted in Figs. \ref{FigLC_TYC8378} and
\ref{FigRV_TYC8378}.

Our analysis of long-term period changes was conducted using all available photometric data.
Fortunately, the star was also found in the database of old photographic plates from German
observatories named APPLAUSE, available online,\footnote{https://www.plate-archive.org/query/} where
the star was observed during the 1960s and 1970s. From that photometry we were able to derive (albeit
with poor precision) the times of several eclipses. These data are highly important for constraining the
value of the long apsidal period with a higher degree of statistical confidence. In total, we collected
19 primary and 19 secondary times of eclipses for the analysis, covering a time span of more than 50
years. However, as seen from the $O-C$ diagram in Fig. \ref{OCdiagrTYC8378}, the change in the omega
angle is still very small and, accordingly, the apsidal motion is very slow. Our estimation of the
period of apsidal motion is on the order of 1000 yr. Our resulting eccentricity value is 0.193, only
slightly different from the value that was published by \cite{2014MNRAS.441..343S}, who presented the
system's orbital eccentricity as $0.17 \pm 0.065$, and from our former value published in
\cite{2018A&A...619A..85Z}.

 \begin{figure}
   \centering
   \includegraphics[width=0.49\textwidth]{LC_OK_TYC8378_uprav.png}
   \caption{Light curves of TYC 8378-252-1.}
   \label{FigLC_TYC8378}
  \end{figure}

  \begin{figure}
   \centering
   \includegraphics[width=0.49\textwidth]{RV_TYC8378.png}
   \caption{Radial velocity curves of TYC 8378-252-1. The red curve applies to the primary component; the black curve applies to the secondary component.}
   \label{FigRV_TYC8378}
  \end{figure}

\begin{figure}
  \centering
  \includegraphics[width=0.49\textwidth]{ASAS185951.png}
  \caption{O-C diagram for the system TYC 8378-252-1.}
  \label{OCdiagrTYC8378}
\end{figure}

\begin{figure}
  \centering
  \includegraphics[width=0.49\textwidth]{ASAS185951_Residuals.png}
  \caption{O-C diagram of residuals for the system TYC 8378-252-1 after subtracting the apsidal motion fit.}
  \label{OCdiagrTYC8378resid}
\end{figure}

\section{Discussion and conclusions}

In the present era of large-scale photometric and spectroscopic surveys, the question arises of whether a
dedicated study of one particular system is  sufficient  to produce results of
astrophysical importance. We answer in the affirmative. Currently, of the more than two million   known
eclipsing binary systems \citep{2006SASS...25...47W, 2022arXiv221100929M}, only 288 systems have had
their physical parameters derived to better than 2\% accuracy \citep{2015ASPC..496..164S}. Only a small
proportion of these systems are eccentric systems. Additional statistics to augment the small
present sample of eccentric systems, in the form of the P-e diagram that depicts the progress of
circularization in binary systems, would provide much-needed insight into the physical processes
occurring in stellar interiors, and into the orbital dynamics. We are therefore confident that this
study makes an important contribution to building the statistics of well-studied eccentric systems
showing apsidal motion.

\subsection{Absolute parameters}
\label{absolute_parameters}

The absolute parameters of binary stars are generally obtained by combining the information contained
in spectroscopic and photometric data and using the appropriate laws of physics. As a first step, the
masses of the components are calculated from Kepler's third law. The fractional radii of the components
($r_1$, $r_2$), obtained from the photometric data, are used to derive the absolute radii ($R_1$,
$R_2$). Subsequently, surface gravities ($g_1$, $g_2$) are derived directly. Using the effective
temperatures listed in Table \ref{abs_par}, we computed the bolometric magnitudes ($M_{\rm bol}$) and
luminosities ($L$) of the component stars of the two systems considered in the present study. We used
the nominal set of solar values   adopted by IAU 2015 Resolutions B2 and B3 as input in our
calculations. The absolute visual magnitudes $M_V$ were derived from the bolometric correction formula,
$BC$ = $M_{\rm bol}$ -- $M_{V}$. Bolometric corrections for the components were taken from the online
version of the color tabulation of \citet{Pecaut_Mamajek_2013}, according to their effective
temperatures.

The distance to each system was calculated from the well-known adaptation of Pogson's law: $M_{V}$ =
$m_{V}$ + 5 -- 5log$(d)$ -- $A_{V}$. The interstellar absorption and intrinsic color index were
computed using the following method. First, the total absorption towards the system in the galactic
disk in the $V$ band, $A_{\infty}(V)$, was taken from \citet{Schlafly_Finkbeiner_2011}, using the NASA
Extragalactic Database\footnote{ http://ned.ipac.caltech.edu/forms/calculator.html}. Second, the
interstellar absorption corresponding to the distance to the system, $A_{d}(V)$, was derived from the
formula given by \citet{Bahcall_Soneria_1980} (in their Eq.~8), using the system's Gaia-DR3 parallax
\citep{Gaia_2022}. Finally, the color excess for the system at the distance $d$ was estimated as
$E_{d}($B$-$V$)$ = $A_{d}(V)$/3.1.

The distance to TYC 5378-1590-1 (with corrections for interstellar absorption) was computed as 728
$\pm$60 pc using the distance modulus. When interstellar absorption was ignored, the distance was
computed as 1110 $\pm$80 pc. The photometric parallax formulation of \citet{Budding_Demircan_2007}
produces a distance of $1050 \pm80$ pc. However, considering the distance provided by Gaia-DR3
\citep{Gaia_2022}, 1292 $\pm$39 pc, the interstellar absorption for TYC 5378-1590-1 thus appears to be
overestimated. This would be in agreement with only low extinction towards the star as derived by
\cite{2020AJ....159...84B}. The  different effective temperatures of the component stars    play
a marginal role.

For TYC 8378-252-1, the distance was calculated as $550 \pm$40 pc when interstellar absorption was
taken into account, and  was calculated as 580 $\pm$50 pc when interstellar absorption was
ignored. The photometric parallax formulation of \citet{Budding_Demircan_2007} produces a distance of
$490 \pm60$ pc. The Gaia-DR3 \citep{Gaia_2022} distance for this star is provided as 670 $\pm$10 pc,
which is somewhat larger than the distance values calculated from the photometric data. As for the
previous case, we can speculate about slightly incorrect extinction or, on the contrary, our results
may be affected by larger errors than presented.

The absolute parameters of TYC 5378-1590-1 and TYC 8378-252-1 as determined by our analysis, together
with their errors, are listed in Table \ref{abs_par}.

\begin{table*}
  \centering
\caption{Absolute parameters of TYC 5378-1590-1 and TYC 8378-252-1.} \label{abs_par}
\begin{tabular}{lllll}
\hline \hline
& \multicolumn{2}{c}{TYC 5378-1590-1} & \multicolumn{2}{c}{TYC 8378-252-1}  \\
Parameter       & Primary       & Secondary & Primary       & Secondary     \\
\hline \hline
$a$ (R$_{\odot}$)       & \multicolumn{2}{c}{15.88 $\pm$0.07}   & \multicolumn{2}{c}{11.39 $\pm$0.15} \\
$M$ (M$_{\odot}$)       & $2.09 \pm0.06$    & $1.78 \pm0.05$    & $1.12 \pm0.06$    & $1.28 \pm0.11$ \\
$R$ (R$_{\odot}$)       & $1.96 \pm0.05$    & $1.69 \pm0.06$    & $1.58 \pm0.07$    & $1.80 \pm0.06$ \\
log $\{g$ (cm s$^{-2}$)$\}$     & $4.17 \pm0.06$    & $4.23 \pm0.07$    & $4.09 \pm0.07$    & $4.04 \pm0.08$ \\
$T$ (K)             & $9800 \pm200$ & $8824 \pm180$ & $6308 \pm210$     & $6600 \pm200$ \\
log $\{L$ (L$_{\odot}$)$\}$     & $1.50 \pm0.06$    & $1.19 \pm0.07$    & $0.55 \pm0.10$    & $0.74 \pm0.08$ \\
$M_{\rm bol}$ (mag)         & $0.98 \pm0.14$    & $1.76 \pm0.17$    & $3.36 \pm0.24$    & $2.88 \pm0.20$ \\
$M_{V}$ (mag)           & $1.21 \pm0.14$    & $1.83 \pm0.17$    & $3.39 \pm0.24$    & $2.90 \pm0.20$ \\
$E$($B$-$V$) (mag)  & \multicolumn{2}{c}{0.30}      & \multicolumn{2}{c}{0.04} \\
$B$-$V$ (mag)       & \multicolumn{2}{c}{0.01 $\pm$0.09$^{a}$}  & \multicolumn{2}{c}{0.60 $\pm$0.18$^{a}$} \\
$V$ (mag)           & \multicolumn{2}{c}{10.95 ~$\pm$0.07$^{a}$}    & \multicolumn{2}{c}{11.18 ~$\pm$0.12$^{a}$} \\
$M_{V}$ $(system)$ (mag)    & \multicolumn{2}{c}{$0.72 ~\pm$0.17}   & \multicolumn{2}{c}{$2.37 ~\pm$0.18} \\
$d$ (pc)                & \multicolumn{2}{c}{728 $\pm$60}       & \multicolumn{2}{c}{550 $\pm$40} \\
$d_{Gaia-DR3}$(pc)  & \multicolumn{2}{c}{1292 $\pm$39$^{b}$}    & \multicolumn{2}{c}{670 $\pm$10$^{b}$} \\
\hline
\end{tabular}
\begin{flushleft}
\item \textit{Notes:} $^{a}$ \citet{Hog_etal_2000};  $^{b}$ \citet{Gaia_2022}.
\end{flushleft}
\end{table*}

\subsection{Evolutionary status}
\label{evolution}

The Granada \citep[e.g.,][]{Claret_2006} and Padova \citep[e.g.,][]{Bressan_etal_2012} evolution models
were used to study the evolutionary status of these two eccentric binary systems, using the physical
parameters listed in Table \ref{abs_par}. The log $T$ versus log $g$ diagram and the log $T$ versus log $L$
diagram (i.e., the H-R diagram) were used to determine the metallicity values $Z$ of the component stars,
whereas the log (age) versus radius diagram and the H-R diagram were used to determine their ages.

In Figs. \ref{evol1} and \ref{evol2}, we display the evolutionary tracks of the component stars that
correspond to their measured masses. The positions of the component stars indicated in the log $T$ versus
log $g$ diagram and in the H-R diagram correspond to values of the metallicity $Z$ for TYC 5378-1590-1
and TYC 8378-252-1 of $Z=0.010\pm 0.001$ and $0.007\pm 0.002$, respectively.

The evolutionary progression of the radii of the components of TYC 5378-1590-1 in accordance with
their determined masses and $Z=0.010$ are displayed in the middle panel in Fig. \ref{evol1}. The
positions of the components are plotted according to their radii,  as listed in Table \ref{abs_par}. The
calculated radius of the primary component corresponds to a log(age)=8.72 and the calculated radius of
the secondary component corresponds to a log(age)=8.83. In the H-R diagram (lower panel
of Fig. \ref{evol1}), the positions of the components determined according to their calculated physical
parameters fit the isochrone of log(age)=8.73  within the error limits. We assigned the value
log(age)=$8.73\pm 0.07$ to TYC 5378-1590-1 (i.e., an age of $537\pm55$ Myr). This value for the age
implies that the theoretical model predicts a smaller radius than the observational radius of the
secondary component, as shown in the radius evolution diagram of the component stars (displayed in the
middle panel of Fig. \ref{evol1}).

The evolutionary progression of the radii of the components of TYC 8378-252-1 in accordance with
their determined masses and $Z=0.007$ are displayed in the middle panel in Fig. \ref{evol2}. The
positions of the components are plotted according to their radii, as listed in Table \ref{abs_par}. The
calculated radius of the primary component corresponds to a log(age)=9.71 and the calculated radius of
the secondary component corresponds to a log(age)=9.50. According to the H-R diagram in the lower panel
of Fig. \ref{evol2}, the positions of the components determined according to their calculated physical
parameters fit the isochrone of log(age)=9.60 within the error limits. We assigned the value
log(age)=$9.60\pm 0.15$ to TYC 8378-252-1 (i.e.,  an age of $3.98 \pm0.80$ Gyr). This value for the
age implies that the theoretical model predicts a smaller radius than the observational radius for the
primary component (the less massive component, as explained above), as shown in the
radius evolution diagram of the component stars (displayed in the middle panel of Fig. \ref{evol2}).

\begin{figure}
\centering
    \includegraphics[scale=1.2]{tyc5378_z.pdf} \\
    \includegraphics[scale=1.2]{tyc5378_age.pdf} \\
    \includegraphics[scale=1.2]{tyc5378_hr.pdf}
\caption{ Location of the components of TYC 5378-1590-1 in the log ($T_{\rm eff}$)--log ($g$) diagram
(upper panel), log (age)--radius diagram (middle panel), and H-R diagram (lower panel). The Granada
evolutionary tracks from ZAMS to TAMS \citep{Claret_2006} for stars of 2.09 M$_{\odot}$ (blue
line) and 1.78 M$_{\odot}$ (red line), corresponding to the primary and secondary stars,
respectively, are displayed for $Z=0.010$ in all panels. The middle panel displays the radial evolution
of the component stars. As discussed in the text, the age of TYC 5378-1590-1 was estimated as
$537\pm55$ Myr. The Padova isochrone line for an age of 537 Myr \citep{Bressan_etal_2012} is indicated
by the dashed black curve superimposed on the H-R diagram. In all diagrams, filled and open circles
 represent the primary and secondary components, respectively. The vertical and horizontal lines are the
error bars of the measured quantities. } \label{evol1}
\end{figure}

\begin{figure}
\centering
\includegraphics[scale=1.2]{tyc8378_z.pdf}
\includegraphics[scale=1.2]{tyc8378_age.pdf}
\includegraphics[scale=1.2]{tyc8378_hr.pdf}
\caption{ Location of the components of TYC 8378-252-1 in the log ($T_{\rm eff}$)--log ($g$) diagram
(upper panel), log (age)--radius diagram (middle panel), and H-R diagram (lower panel). The Granada
evolutionary tracks from ZAMS to TAMS \citep{Claret_2006} for stars of 1.12 M$_{\odot}$ (blue
line) and 1.28 M$_{\odot}$ (red line), corresponding to the primary and secondary stars,
respectively, are displayed for $Z=0.007$ in all panels. The middle panel displays the radial evolution
of the component stars. As discussed in the text, the age of TYC 8378-252-1 was estimated as $3.98
\pm0.80$ Gyr. The Padova isochrone line for an age of 3.98 Gyr \citep{Bressan_etal_2012} is indicated
by the dashed black curve superimposed on the H-R diagram. In all diagrams, filled and open circles
  represent the primary and secondary components, respectively. The vertical and horizontal lines are the
error bars of the measured quantities. } \label{evol2}
\end{figure}

\subsection{Internal structure constant}
\label{isc}

In this section we describe the results of our calculations of the internal structure constants of
these two eccentric binary systems, using the method and equations given by \citet{Claret_etal_2021}
and references therein.

The observational apsidal motion rates $\dot{\omega}_{obs}$ were derived from the $O-C$ analysis in
Section \ref{analysis}, as $0.000368 \pm0.000112$  deg cycle$^{-1}$ for TYC 5378-1590-1 and $0.002852
\pm0.000851$  deg cycle$^{-1}$ for TYC 8378-252-1.

The relativistic term in the rate of apsidal motion was calculated using the following equation, which
was described by \citet{Levi-Civita_1937} and presented by \citet{Gimenez_1985}:
\begin{equation}
\dot{\omega}_{rel}=5.447\times10^{-4}\dfrac{(M_{1}+M_{2})^{2/3}}{(1-e^{2})P^{2/3}} \qquad
(\textrm{deg\:cycle$^{-1}$}). \label{omega_rel}
\end{equation}
Here $M_{1}$ and $M_{2}$ represent the masses of the component stars in solar units, $e$
the orbital eccentricity, and $P$   the orbital period in days. Subsequently, the relativistic
terms were calculated as $0.000615 \pm0.000056$ deg cycle$^{-1}$ for TYC 5378-1590-1 and $0.000500
\pm0.000044$ deg cycle$^{-1}$ for TYC 8378-252-1.

There is a remarkable result here for TYC 5378-1590-1. If we extract the classical term
$\dot{\omega}_{cl}$ from the well-known equation
$\dot{\omega}_{obs}$=$\dot{\omega}_{cl}$+$\dot{\omega}_{rel}$, the term $\dot{\omega}_{cl}$   takes a
negative value since $\dot{\omega}_{rel} > \dot{\omega}_{obs}$. This  scenario is often encountered in
eclipsing binary systems with a very slow rate of apsidal motion \citep[e.g.,][]{Gimenez_1985}. The most
famous of these examples is the system DI Her  \citep[e.g.,][]{Guinan_Maloney_1985}.
\citet{Albrecht_etal_2009} observationally demonstrated that this phenomenon in DI Her is caused by
misaligned spin and orbital axes of the component stars (see also \citealt{1985SvAL...11..224S}). We
were not able to perform a similar procedure in order to show whether there is spin-axis misalignment
in the components of TYC 5378-1590-1 because of our lack of access to high-resolution spectra taken at
the conjunction phases of this system.

The classical term was derived as $\dot{\omega}_{cl}=0.002352 \pm0.000732$ deg cycle$^{-1}$ for TYC
8378-252-1, contributing approximately 82$\%$ of the observed rate of apsidal motion. Using the absolute
parameters   listed in Table \ref{abs_par}, the mean observational internal structure constant of this
system was calculated as $\log{\bar{k}_{2,obs}}=-2.728 \pm{0.120}$.

The theoretical internal structure constants $\bar{k}_{2,theo}$ were predicted from the Granada
evolution models \citep{Claret_Gimenez_1992,Claret_2006}. The Granada models produce theoretical values
of $\log{k_{2}}$ for a grid of masses, surface gravities, luminosities, effective temperatures, ages,
and metallicities. Values of $k_{2i}$ for each component star were calculated by interpolating between
the model values and the observed physical properties listed in Table \ref{abs_par}.

The predicted metallicities and ages of TYC 5378-1590-1 and TYC 8378-252-1 based on our analysis of
Granada models are summarized in Table \ref{ics_par}. These results were also checked against the
Padova and Geneva models. Using the absolute parameters given in Table \ref{abs_par} (in accordance with
the masses of the components and the values of $Z=0.010$ and 0.007), interpolating, taking the weighted
average and then the logarithm, the mean observational internal structure constants of TYC 5378-1590-1
and TYC 8378-252-1 were determined as $\log{\bar{k}_{2,theo}}=-2.435 $ and $-2.424 $, respectively,
from the Granada Models. These values are given in Table \ref{ics_par} for ease of comparison of the
observational and theoretical values.

\begin{table}
  \centering
\caption{Metallicities, observational and theoretical internal structure constants, and evolutionary
and circularization ages of TYC 5378-1590-1 and TYC 8378-252-1.} \label{ics_par}
\begin{tabular}{lll}
\hline
Parameter & TYC 5378-1590-1 & TYC 8378-252-1  \\
\hline

$Z$                     & 0.010 $\pm$0.001      & 0.007 $\pm$0.002 \\
log $\bar{k}_{2,obs}$       & ---                   & $-2.728 \pm0.120$  \\
log $\bar{k}_{2,theo}$      & $-2.435$          & $-2.424$ \\
Age (yr)                    & $(5.37 \pm0.55) \times 10^8$      & $(3.98 \pm0.80) \times 10^9$  \\
$\tau_{circ}$ (yr)          & $1.10 \times 10^{11}$ & $2.76 \times 10^8$ \\
\hline
\end{tabular}
\end{table}

For TYC 5378-1590-1, log $\bar{k}_{2,obs}$ could not be calculated because the term $\dot{\omega}_{cl}$
is negative, as mentioned before, and therefore this parameter could not be entered in Table \ref{ics_par}.
As an approach to solving this problem, we started by accepting the expected result (i.e., log
$\bar{k}_{2,obs}$ = log $\bar{k}_{2,theo}$) and used the equations given by \citet{Claret_etal_2021} to
calculate the classical apsidal motion rate as $\dot{\omega}_{cl}$ = 0.00199 deg cycle$^{-1}$ (hence,
the period of apsidal motion as $U = 1410$ yr). Upon entering these values as input values to the $O-C$
analysis and repeating the iterations, we obtained $\dot{\omega}_{obs} = 0.00261 \pm0.00091$ deg
cycle$^{-1}$ (and $U = 1409.5 \pm361.7$ yr). Calculations of other parameters resulted in the same
values as those listed in Table \ref{am_parameters}, within the error limits. Thus, in the $O-C$
analysis of TYC 5378-1590-1, two different models appeared for the apsidal motion of the system: Model
A with a long period of apsidal motion ($U=9937$ yr, $rms = 0.0023$), and Model B with a short period
of apsidal motion ($U=1410$ yr, $rms = 0.0064$). In the comparison of these two models, while the $rms$
values point to Model A as the most likely solution, the negative result of the classical term in this
model creates a problem similar to the situation in DI Her. However, the fact that the $rms$ values
between these two models are not very different in terms of statistical significance prevents a
definitive determination of the most realistic model from being made. In addition, the fact that the periods
of apsidal motion in both models are on the order of a thousand years implies that a sufficient number of
eclipse times could only be obtained in a few centuries to indicate which model is correct. Therefore,
the solution to this problem for TYC 5378-1590-1 remains open-ended for the time being.

For TYC 8378-252-1, the value of $\log{\bar{k}_{2,theo}}$ predicted from the Granada models  was
approximately 11$\%$ larger than the observed value (that is, by $1\sigma$). In comparing the values of
$\log{\bar{k}_{2,obs}}$ and $\log{\bar{k}_{2,theo}}$, the absolute parameters derived from the
observations are expected to be compatible with those of the evolution models and to indicate the same age
for both components of a given binary star. In the case of TYC 8378-252-1 (see Sect.
\ref{evolution}), in Fig. \ref{evol2}, for the less massive primary component, the upper and lower
panels show that the evolution model predicts a temperature value greater than the observational value
within the margins of error, while the middle and lower panels show that the evolution model
predicts a smaller radius than the observational value. Although the age determination in the H-R
diagram is accepted as log(age)=9.60 within the error limits, the middle panel also shows that the
measured radii of the component stars indicate different ages for the system.

\citet{Lester_Gies_2018} pointed out that the mismatch between the observational and theoretical radii
of these component stars (which translates to incompatible ages for the components) is encountered for
for evolved F-type eclipsing binary components similar to TYC 8378-252-1. As \citet{Lester_Gies_2018} mentioned, convective cores have started developing in evolved F-type stars, given their mass in the range of 1.1--1.7 Msun, and given that convective core overshooting disturbs central condensation. This situation is not adequately represented in current evolution models. For example, in the case of the TYC 8378-252-1
system, the evolution model gives an internal structure constant larger than the observational value,
which indicates that the components are more centrally condensed than predicted by models.

The evolutionary age of TYC 8378-252-1, which has a remarkably eccentric orbit ($e \sim 0.2$), is quite
large, and both components appear to have evolved almost to the TAMS as main-sequence stars. This casts
doubt on whether the expected orbit-circularization mechanism has been operating in this system. To
investigate this problem, the circularization timescale was calculated using the \citet{Zahn_1977}
theory.

Considering the spectral types (and effective temperatures) of the components of TYC 8378-252-1 (see
Section \ref{tyc8378}), it can be accepted that these stars have convective envelopes. In this case,
using Eq. (6.2) in \citet{Zahn_1977} for stars with convective envelopes and the corresponding absolute
parameters in Table \ref{abs_par} (above), the circularization timescale was calculated as $\tau_{circ}
= 2.76 \times 10^{8}$ yr. Comparing the results in Table \ref{ics_par}, since the evolutionary age of
TYC 8378-252-1 is approximately ten times older than its circularization age, this binary system would
  be expected to have a circular orbit at present. Therefore, our results are not compatible with
the predictions of the \citet{Zahn_1977} theory of circularization.

The spectral types of the components of TYC 5378-1590-1 (see Section \ref{tyc5378}) indicate that these
stars should have convective cores and radiative envelopes. Therefore,  the \citet{Claret_Cunha_1997}
formulation of the \citet{Zahn_1977} theory for stars with convective cores and radiative envelopes
was used to find the circularization timescale of TYC 5378-1590-1. The tidal torque constant $E_2$ and
fractional gyration radius $R_{gyr}$  in the formulas were determined by interpolating, according to
the mass and surface gravity of the component stars, from the Granada evolution models
\citep{Claret_2006}. Using $\log (E_{21}) = -7.008$, $R_{gyr,1}=0.198$ and $\log (E_{22}) = -7.557$,
$R_{gyr,2}=0.199$ for the primary and secondary components of TYC 5378-1590-1 and the absolute
parameters listed in Table \ref{abs_par}, the equations of \citet{Claret_Cunha_1997} predict the
circularization timescale to be $\tau_{circ} = 1.10 \times 10^{11}$ yr. As a result, the
circularization age of TYC 5378-1590-1 is approximately 200 times older than its evolutionary age and
the orbit of the system is still eccentric, which shows that the observational findings for this system
agree with the  \citet{Zahn_1977} theory of circularization.

\begin{acknowledgements}

This research was supported by T\"{U}B\.{I}TAK (Scientific and Technological Research Council of
T\"{u}rkiye) under Grant No. 121F203. We would like to thank the Time Allocation Committee of the SAAO
for ample observing time. CE and FM thank the National Research Foundation of South Africa and the
University of Johannesburg for funding. Funding for APPLAUSE has been provided by DFG (German Research
Foundation, Grant), Leibniz Institute for Astrophysics Potsdam (AIP), Dr. Remeis Sternwarte Bamberg
(University Nuernberg/Erlangen), the Hamburger Sternwarte (University of Hamburg) and Tartu
Observatory. Plate material also has been made available from Th\"uringer Landessternwarte Tautenburg.

It is a pleasure to express our appreciation of the high quality and ready availability, via the
Mikulski Archive for Space Telescopes (MAST), of data collected by the TESS mission. Funding for the
TESS mission is provided by the NASA Explorer Program. The authors thank the ASAS, ASAS-SN, CRTS, NSVS
and TESS teams for making all of the observations easily public available. This research has made
partial use of data from the European Space Agency (ESA) mission {\it Gaia}
(\url{https://www.cosmos.esa.int/gaia}), processed by the {\it Gaia} Data Processing and Analysis
Consortium (DPAC, \url{https://www.cosmos.esa.int/web/gaia/dpac/consortium}). Funding for the DPAC has
been provided by national institutions, in particular the institutions participating in the {\it Gaia}
Multilateral Agreement. This research has partly made use of the SIMBAD and VIZIER databases, operated
at CDS, Strasbourg, France, and of NASA's Astrophysics Data System Bibliographic Services.

 \end{acknowledgements}

redpajama_set_name: RedPajamaArXiv


text:
Q: JavaScript dynamically updating total and quantity totals For some reason when I update the quantity the total price changes to the total price of which every input I choose. The price won't update properly in the different subtotals either, the second one thinks it is 29.95. And then I can't get the quantity to update properly either. Here is a demo I'm using: http://jsfiddle.net/656arnLy/

<input type="number" min="0" class=" qty form-control" id="quantity">
<input type="text" class="price form-control" id="price" value="29.95" readonly>
<input type="text" class="subtotal form-control" id="subTotal">

<input type="number" min="0" class=" qty form-control" id="quantity">
<input type="text" class="price form-control" id="price" value="2.99" readonly>
<input type="text" class="subtotal form-control" id="subTotal">

Total Price:
<input type="text" readonly class="totalPrice" id="total">

Total qty:
<input type="text" readonly class="totalQty" id="total">

$(function () {
$(".qty").change(function () {
    var qty = $(this).hasClass('qty') ? $(this).val() : $(this).siblings('.qty').val();
    var price = $(this).hasClass('price') ? $(this).val() : $(this).siblings('.price').val();
    price = price || 0;
    qty = qty || 0;
    var subtotal = price >= 1 && qty >= 1 ? parseFloat(price * qty) : 0;
    $(this).siblings('.subtotal').val(subtotal);
    var totalPrice = 0;
    var totalQty = 0;
    var update = false;
    $('.subtotal').each(function () {
        subtotal = parseFloat($(this).val()) | 0;
        totalPrice = subtotal ? (parseFloat(totalPrice + subtotal)) : totalPrice;
    });
    $('.qty').each(function () {
        qty = $(this).val();
        totalQty += qty;
    });
    $('.totalPrice').val(totalPrice);
    $('.totalQty').val(totalQty);
});

Update: I got the total to work correctly, I just can't get the quantity to work. And are there ways to get around using  so I can put this code for each row in a table??
Updated site: http://jsfiddle.net/656arnLy/14/

A: Just scanning through your code, several of your input boxes have the same id value. You have two inputs with id value "quantity", 2 with id value price and so on. You definitely do not want to do this. This can cause all sorts of issues. Also, you're updating all inputs that have classname .subtotal in the $(this).siblings line.
Give your inputs different id values, and select the id you want to update and you'll be closer to what you want.

redpajama_set_name: RedPajamaStackExchange


"...[A]ll the music I assembled for this recording was intended to inspire or allude to dancing; albeit maybe an abstract style," says drummer Mike Reed in the liner notes to A New Kind of Dance.
Sure enough, Reed launches the title track and the sixth People, Places & Things album with a swinging, syncopated-funk backbeat. It won't be mistaken for an attempt at mainstream jazz, though, since the tune also has pianist Matthew Shipp sitting in with the Chicago group, stretching and rolling over his keys. In fact it takes a few measures to find the One in Reed's groove. Right as that happens, saxophonists Greg Ward (alto) and Tim Haldeman (tenor) fire the staccato theme of the head and disappear just as quickly, letting Shipp take the first solo.
Shipp and trumpeter Marquis Hill each join the quartet (which includes bassist Jason Roebke) on a set that splits evenly between Reed compositions and a few well-picked covers that reach beyond the group's original source of inspiration. The results yield a set that shifts gears on every track without letting the energy or focus wane. It indeed can inspire dancing, if only in your head.
The group follows the opener with "Markovsko Horo," a traditional Bulgarian folk dance that sounds like rubato klezmer music. Hill adds color to the music that recalls Don Cherry's tartness. Rather than opening it up for solos, Reed ingeniously cuts it short, wrapping up after the theme and an accelerando that gives the horns a few quick moments to blow. The music goes to South Africa for the bright "Kwela for Taylor," written by reedist Michael Moore (of ICP, Clusone Trio and others). The late South African musician Sean Bergin is remembered with his "AKA Reib Letsma," where the backbeat gets even more pronounced and the saxophonists blow in unison and in shrieks of joy that dance around each other. The only problem with this track comes with the abrupt ending, right as Roebke and Reed seemed to be getting into a heavy breakdown.
Before they get to that number, they also do some serious business to "Fear Not of Men," originally done by the rapper Mos Def, and "Star Crossed Lovers," an Ellington/Strayhorn number in which Ward, Haldeman and Hill are left on their own for two minutes, largely playing off the theme, with gentle backing from Roebke.
As good as the interpretations sound, Reed's own writing should not be overlooked. "Candyland," Ornette-ish in both the theme's delivery and brevity, brings out the best of the quartet with some blowing that sounds like a throwback to the original era of the New Thing - complete with new excitement. Both do the same on the free-wheeling "Wonderland." Shipp gets his Andrew Hill on in "Jackie's Tune," stopping you in your tracks to consider where these great ideas are coming from.
To make a short story long, there isn't a dud on this album. Far from it.
I need new glasses. Badly. Thanks. Correction has been made.


text:
« John Kannenberg Says Goodbye to Chicago (MP3s)
Quote of the Week: Sale-less Record Shop »
Chris Carter (Throbbing Gristle) Radiophonic Workshop Tribute MP3
[ May 22, 2009 / Department: downstream / Leave a comment ]
Just this morning, Chris Carter of Throbbing Gristle uploaded a free MP3 to the excellent audio-showroom service that is soundcloud.com. At his soundcloud.com/chris_carter page, there are now two free files available, the most recent of which is "Experimental Tribute" (MP3). It's a rousing whorl of noise, deep thick echoes of counter-posed wave forms, and otherworldly sonic churn, atop a series of slowly alternating pulses.
[audio:http://media.soundcloud.com/chris_carter/experimental-tribute/download|titles="Experimental Tribute"|artists=Chris Carter]
If the whole thing sounds like the score to some 1960s sci-fi B-movie, the reason may be that what the track is a tribute to is the BBC Radiophonic Workshop, source of all forms of sonic experimentation (notably the eerie sounds of Dr. Who), and which would have turned 50 this year had it not been shuttered a decade ago.
Carter's track also represents a fascinating aspect of Internet-based music, in that the recording is a real-time reaction by an artist to the news. The Workshop's been the subject of anniversary reflections this week (bbc.co.uk, disquiet.com). We're already used to seeing musicians, and other artists (and, more generally, public figures), blur the line between public and private online (Carter himself announced the track via his twitter.com/chriscarter account). Musicians giving us peeks into their studios and lives is one thing, but witnessing them respond to the world in a diary-like musical mode is something altogether more promising.
Carter has also posted video of the performance that led to the MP3 (at vimeo.com and flickr.com — from which the above still image was taken).
In addition, at three of those four web-based communal spaces (Vimeo, Flickr, and SoundCloud — and, soon enough, no doubt, in Twitter), Carter is conversing with commenters about the track. One of the early comments on the Vimeo thread is Carter's fellow British musician Scanner, whom Twitter followers have seen communicating with Carter in recent weeks. Jokes Scanner, in reference to the array of effects involved in making "Experimental Tribute": "Great fun there Chris (just hope you weren't running on batteries!)"
[ Tags: free, live-performance, software, video / Leave a comment ]

redpajama_set_name: RedPajamaCommonCrawl


text:
Places to Visit around New York, Ny/US/
Kenley Common
Croydon, United Kingdom
Kenley Common, owned and manged by the City of London at no cost to the public, is a 56Ha (139acre) public open space. Located in the London Borough of Croydon, it forms part of a larger area of open countryside within the London Green belt that links London with...
64.5 miles Open Space
Vintage Trains
670 Warwick Road, Tyseley, Birmingham, West Midlands, B11 2HL, United Kingdom
One of the U.K.'s leading operators of main line steam train excursions. We have a varied year-round tour programme of steam railway trains and some classic modern traction tours all run on the Network Rail network. During the summer we operate the Sundays-only...
120.7 miles Other
American Museum In Britain
Claverton Manor, Bath, Somerset, BA2 7BD, United Kingdom
The American Museum in Britain is home to a unique collection, in a breathtaking setting. There is something for everyone to enjoy at the only museum of Americana outside the United States.
221.2 miles Museum
Dumbarton Castle
Dumbarton Castle, Strathclyde, United Kingdom
Dumbarton Castle guards the point where the River Leven joins the River Clyde. Its recorded history reaches back 1,500 years. At that time the place was known as Alt Clut, 'Rock of the Clyde'. Later it became known by the Gaelic name Dun Breatann, 'Fortress of...
506.0 miles Historic House
Museum of Domestic Design & Architecture
9 Boulevard Drive, Beaufort Park, London, NW9 5HF, United Kingdom
The Museum of Domestic Design & Architecture's (MoDA) collections are available Online, On Tour and On Request. The collections include wallpapers, textiles, designs, books, catalogues and magazines from the late nineteenth to the late twentieth century. They are...
Kettle's Yard House and Gallery
Kettle's Yard Castle Street, Cambridge, CB3 0AQ, United Kingdom
On Castle Street in Cambridge, is a beautiful and unique house containing a distinctive collection of modern art. * Please note that during 2012/13, Kettle's Yard is commencing construction of a new Education Wing to meet the expanded needs of our education...
673.3 miles Art Gallery
Matt's Gallery
42–44 Copperfield Road, London, E3 4RR, United Kingdom
The intention of Matt's Gallery is to provide artists with the space and time to develop new ideas and possibly new ways of working while making a new work for the space in which it is to be exhibited. In this way it was hoped to provide the best possible...
Little Chester Heritage Centre
St Paul's Church Chester Green Mansfield Road, Derby, Derbyshire, United Kingdom
The Centre shows the history of Little Chester (Chester Green) from Roman to recent industrial times by means of artefacts, models and photographs.
Yorkshire Wildlife Trust - Flamborough Cliffs
Flamborough, United Kingdom
Flamborough Cliffs is a coastal reserve, ranging from cliff top grassland and spectacular chalk cliffs to rocky shore and sandy beach. It is a wonderful reserve on which to see huge numbers of breeding seabirds, species rich grassland, farmland birds and a variety...
943.8 miles Open Space
Yorkshire Wildlife Trust - Ashkam Bog
Askham Bog, the oldest and perhaps most prestigious Trust reserve is renowned for its ancient relict fen and bog flora and fauna, a rare and extraordinary combination. Askham Bog is a unique meeting place for wetland plants and animals from the south and east on one...
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Cheap places to visit in Bergenfield


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DYING WISH - Gives Voice To Survivors With New Single "Severing The Senses"
Portland-based blistering hardcore five-piece Dying Wish have unveiled their pummeling new track "Severing The Senses" today. Dying Wish align themselves with the continuing battle for liberation, encompassing the issues affecting BIPOC, the environment, policing and more intersectional causes while dealing in personal tribulation and trauma in equal measure. They make music aimed at unity but without compromise and this single does just that as a song for survivors.
"I wrote the lyrics at a time when friends of mine were coming forward about their experiences with abuse after years of their stories being invalidated and suppressed. As a survivor myself, it was triggering for me to see their bravery met with even more denial and excuses from the person who caused them harm. That feeling of anger and sadness I get in those moments will forever be unparalleled. 'I cannot escape this torment granted by the hand of a coward' is specifically about those triggered emotions", lead vocalist Emma Boster shares on the new single. She continues: "After growing up in a home where I experienced violence, I had a very distorted expectation from men. As a result, I found myself in a relationship where I experienced other forms of abuse. 'I felt the weight of every mistake you made' and 'I took the blame each time you broke my heart' refers to the gaslighting and manipulation I dealt with in my first relationship. It's a story I no longer tell because of how many times I've been told that my trauma wasn't real. The idea of the letter on the deathbed is intended for the survivor to have the last word so they never have to feel invalidated again".
"Severing The Senses" joins previously released single "Until Mourning Comes" and title track "Fragments of a Bitter Memory" from the band's forthcoming debut album due out October 1, 2021 via Sharptone Records. Pre-orders are available now here.
In less than three years after their formation, and ahead of their debut album, Dying Wish has already been nominated for "Best International Band" at the UK's Heavy Music Awards, as well as have been called, not once, but twice: "one of the best new bands out right now" by Revolver. Brooklyn Vegan has also listed the band's forthcoming album is one of the top most-anticipated releases of 2021.
Get the single: https://shrptn.co/severingthesenses
Fragments of a Bitter Memory Tracklisting:
01. Cowards Feed, Cowards Bleed
02. Hollowed By Affliction
03. Innate Thirst
04. Severing The Senses
05. Fragments Of A Bitter Memory
06. Cold Hearts In Bloom
07. Until Mourning Comes
08. Now You'll Rot
09. Blood Laced Misery
10. Enemies In Red
11. Drowning In The Silent Black


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Q: importing js module executes css file I'm trying to create a single index file that I can import similar modules.
e.g.
import { foo } from './random';
// or
import bar from './random';

so I have index.js file in random/
import bar from './bar';
import foo from './foo';

export {
  foo
};

export default DefaultSurvey;

that works great, however I have a minor issue.
foo.js extends bar.js
import './Foo.scss';
export default class Foo extends Bar

the problem lies here:
import foo from './foo';

If I try import bar from './random';
the css from foo.js applies to the default export., why is that?

A: First of all, why is this a problem? Shouldn't all css be loaded? Unless, you want to conditionally load certain css-files, which is another issue.
Maybe I've got this question all wrong, and please correct me if I have, but when you import the default export from random/, i.e. import bar from './random';, you are also executing all imports in that module i.e. importing all dependencies. Since you are importing foo from './foo'; in the random/-module, and importing the css in foo.js, these dependencies will be loaded when referincing the random/-module.
To avoid a circular dependency hell, I'd recommend putting all imports of css-files into one file, e.g. the index file. That way you could avoid unexpected behaviour.


Promote the home-school connection with our newest resource for your digital citizenship toolkit.
As educators, we know that having our students' families' involvement is essential. And when it comes to something as important as digital citizenship, knowing that our students' families are clued in can have a huge impact on learning-outcome retention and awareness. Developing a strong home-school relationship can promote student learning and engagement as well as ensure that everyone is on the same page.
In looking to help educators promote that home-school connection, we are excited to announce our newest resource, which you can add to your home-school toolbox around digital citizenship. Our new Family Activity Worksheets take inspiration from the beloved Highlights Kids worksheets that always made their way home in our backpacks throughout elementary school.
Aligned to each lesson in our Digital Citizenship Curriculum, the new Family Activity Worksheets look to bring parents and caregivers into the conversation. Families can test their digital citizenship skills together and explore new tips and tricks to getting the most out of their digital lives in a respectful and responsible way. The worksheets are made up of mini-puzzles and fun, quick activities that families can do together in a no-tech, low-tech, or high-tech way. Pair each activity worksheet with its associated lesson, or use them to introduce various topics and ideas to your students and their families at home.
Announcing Digital Citizenship on Nearpod!


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Google simplifies requirements for Instant apps and games, support for app ads coming soon
Martim Lobao
2018/08/21 5:56am PDT Aug 21, 2018
One of the things that's unique to the Play Store compared to other mobile app stores is the ability to try out an app without having to download and install it. Android Instant Apps have been around for over two years now, with support for Instant Games added back in March, allowing potential users to play around with a game before deciding to download the full version. For developers, this provides a golden opportunity to get their app or game into the hands of users who would likely not have downloaded it otherwise, with the only real drawback being the small additional work involved in getting the Instant app up and running.
Facebook Messenger is testing yet more interface changes, with tabs and Instant Games section
We knew changes were incoming for Facebook Messenger after last month's F8 Developer Conference, during which the focus was largely on better discovery of bots and "Chat Extensions" to add those bots into group conversations. Now it seems Facebook is testing new UI changes, including top-level tabs and a games section in the bottom nav bar.


Action Manufacturing Co.,* Bristol, Pennsylvania (W15QKN-18-D-0083); and AMTEC Corp.,* Janesville, Wisconsin (W15QKN-18-D-0084), will compete for each order of the $250,784,252 firm-fixed-price contract to manufacture, inspect, test, package, and deliver M739A1 Point Detonating/Delay Fuzes. Bids were solicited via the Internet with three received. Work locations and funding will be determined with each order, with an estimated completion date of June 28, 2023. U.S. Army Contracting Command, Fort Dix, New Jersey, is the contracting activity.
NCI Information Systems Inc., Reston, Virginia, was awarded a $45,760,099 cost-plus-fixed-fee contract for information technology services for cyber network operations and security support. One bid was solicited with one bid received. Work will be performed in Fort Huachuca, Arizona, with an estimated completion date of June 30, 2019. Fiscal 2018 operations and maintenance, Army funds in the amount of $45,760,099 were obligated at the time of the award. U.S. Army Contracting Command, Aberdeen Proving Ground, Maryland, is the contracting activity (W91RUS-18-C-0017).
Microsoft Corp., Redmond, Washington, was awarded a $13,499,934 firm-fixed-price contract for non-personal consulting services for Enterprise directory, systems management, Army Golden Master sustainment support, SharePoint, and Enterprise service management system. One bid was solicited with one bid received. Work will be performed in Fort Huachuca, Arizona, with an estimated completion date of June 27, 2019. Fiscal 2018 operations and maintenance, Army funds in the amount of $13,499,934 were obligated at the time of the award. U.S. Army Contracting Command, Aberdeen Proving Ground, Maryland, is the contracting activity (W91RUS-18-C-0018).
Tammy Siler, Clairfield, Tennessee, was awarded a $10,999,949 modification (P00005) to contract W9124M-16-D-0006 for paving. Work locations and funding will be determined with each order, with an estimated completion date of June 30, 2019. U.S. Army Mission and Installation Contracting Command, Fort Stewart, Georgia, is the contracting activity.
Huntington Ingalls Industries, Newport News Shipbuilding Inc., Newport News, Virginia, is awarded a not-to-exceed $200,446,196 undefinitized fixed-price, incentive firm target modification to a previously awarded contract (N00024-16-C-2116) for the purchase of additional long lead time material in support of USS Enterprise (CVN 80). Work will be performed in Newport News, Virginia, is expected to be completed by February 2027. Fiscal 2018 shipbuilding and conversion (Navy) funding in the amount of $200,446,196 will be obligated at the time of award and will not expire at the end of the current fiscal year. This contract was not competitively procured. The statutory authority for this sole-source award is in accordance with Federal Acquisition Regulation 6.302-1(a)(2)(iii) - only one responsible source and no other supplies or services will satisfy agency requirements. The Naval Sea Systems Command, Washington Navy Yard, Washington, District of Columbia, is the contracting activity.
GSI Pacific Inc.,* Honolulu, Hawaii, is awarded $12,481,550 for a firm-fixed-price task order (N6247818F4183) under a previously awarded multiple award construction contract (N62478-16-D-4015) to overhaul a dry dock caisson and provide dock repairs at Joint Base Pearl Harbor-Hickam. The work to be performed provides for 10-year ultrasonic testing of the entire caisson in accordance with Military Standard 1625D including, but not limited to, plating of the entire hull, top deck (weather deck), machinery deck, internal strength decks, bulkheads including breast hooks, ballast tank and machinery deck internal structural members such as stiffeners, truss frame members and sea chests/ballast piping seaward of the first closure valve. Other repair scope items include sandblasting and preserving exterior surfaces of the caisson, including the weather deck; cleaning, priming and painting the exterior of the caisson; removing existing non-skid coating from the weather deck and replacing with industrial strength tape applied to non-skid surface material; replacing non-skid coating on the machinery deck and sandblasting, cleaning, priming and painting of the interior surfaces of the caisson utilizing high solids paint for the interior tanks. Work will be performed in Oahu, Hawaii, and is expected to be completed by March 2020. Fiscal 2018 operations and maintenance (Navy) contract funds in the amount of $12,481,550 are obligated on this award and will expire at the end of the current fiscal year. Two proposals were received for this task order. The Naval Facilities Engineering Command, Hawaii, Joint Base Pearl Harbor-Hickam, Hawaii, is the contracting activity.
Lockheed Martin Corp., Lockheed Martin Space, Sunnyvale, California, is awarded an $11,877,482 cost-plus-fixed-fee contract for Hypersonic Booster technology development seeking to demonstrate technologies related to intermediate range capability through booster design, fabrication and validation testing. The work will be performed in Sunnyvale, California (49.34 percent); Magna, Utah (34.16 percent); Elma, New York (10.70 percent); Huntsville, Alabama (3.75 percent); and Mooresville, North Carolina (2.05 percent), with an expected completion date of June 2019. Fiscal 2018 research, development, test, and evaluation funds in the amount of $11,877,482 are being obligated on this award, none of which will expire at the end of the current fiscal year. This contract was a competitive acquisition. Strategic Systems Programs, Washington, District of Columbia, is the contracting activity (N00030-18-C-0025).
Ocean Ships Inc., Houston, Texas, is awarded a $9,691,694 modification for the fixed price portion of a previously awarded contract (N00033-13-C-3333). This modification is for a six-month bridge contract to continue the operation and maintenance of two Expeditionary Transfer Dock ships, USNS Montford Point (T-ESD 1) and USNS John Glenn (T-ESD 2). Work will be performed worldwide, supporting the Navy afloat prepositioning requirements. The contract extension is expected to be completed by Jan, 1, 2019. Working capital contract funds in the amount of $9,415,503 are obligated for the period, and will not expire at the end of the fiscal year. This contract extension was not competitively procured in accordance with Federal Acquisition Regular 6.302-2 and 10 U.S. Code § 2304(c)(2). The Navy's Military Sealift Command, Norfolk, Virginia, is the contracting activity.
Raytheon Co., El Segundo, California, is being awarded $9,027,700 for a firm-fixed-price delivery order (N00039-13-D-0075) under a previously awarded contract (N00039-16-D-0075) for 279 NATO Improved Link Eleven Modernized Link Level Communication Security (COMSEC) LLC 7M production units. The LLC 7M provides a secure COMSEC capability for the Link 22 Tactical Data Link System for U.S. and foreign military platforms. This contract combines purchases for the Navy (approximately 14 percent) and for the governments of Link 22 partner nations (approximately 86 percent) under the Foreign Military Sales program. Work will be performed in El Segundo, California, and is expected to be completed by April 2020. Fiscal 2018 special defense acquisition funding; shipbuilding conversion (Navy); and fiscal 2018 other procurement (Navy) funds in the amount of $9,027,700 will be placed on the delivery order and obligated at the time of award. Contract funds will not expire at the end of the current fiscal year. This contract was not competitively procured because it is a sole-source acquisition pursuant to the authority of 10 U.S. Code 2304(c)(1), one source or limited sources (Federal Acquisition Regulation 6.302-1(a)). The Space and Naval Warfare Systems Command, San Diego, California, is the contracting authority.
Dimensions Construction Inc.,* San Diego, California, is awarded $7,689,264 for a firm-fixed-price task order (N6247318F4566) under a previously awarded multiple award construction contract (N62473-18-D-5819) for the renovation of Bachelor Enlisted Quarters Building 150 at Naval Base Ventura County, San Nicolas Island. The work to be performed provides for repair and replacement of deteriorated flooring, walls, ceiling, doors, windows, soffits, and stairs. Work will also include upgrades to improve energy efficiency for heating, ventilation, and air conditioning, windows, toilets, faucets, and photovoltaic system. This facility will be repaired and modernized to meet current configuration guidance and safety criteria. Work will be performed in Port Hueneme, California, and is expected to be completed by December 2019. Fiscal 2018 operation and maintenance (Navy) contract funds in the amount of $7,689,264 are obligated on this award and will expire at the end of the current fiscal year. Five proposals were received for this task order. The Naval Facilities Engineering Command, Southwest, San Diego, California, is the contracting activity.
Martin-Baker Aircraft Co. Ltd., Uxbridge, United Kingdom (N00104-18-C-K060), is being awarded a $7,687,490 firm-fixed-price contract for the manufacture of 614 explosive cartridge kits; and 943 each of 12 different explosive cartridges used in the Martin-Baker ejection seat in F-35 aircraft for the Joint Strike Fighter program. This announcement involves foreign military sales: Korea (5.19 percent); Israel (3.78 percent); and Japan (3.05 percent). The contract does not contain a provision for an option quantity. Work will be performed in the United Kingdom (85 percent); and Hollister, California (15 percent), and will be completed by February 2020. Fiscal 2018 operations and maintenance (International Partner Funding) (23.50 percent); fiscal 2018 procurement (Air Force) (20.35 percent); fiscal 2018 operations and maintenance (Air Force) (18.85 percent); fiscal 2018 procurement (Marine Corps) (9 percent); fiscal 2018 operations and maintenance (Marine Corps) (7.65 percent); Foreign military sales (FMS) Korea (5.19 percent); fiscal 2018 operations and maintenance (Navy) (4.36 percent); fiscal 2018 procurement (Navy) (4.27 percent); FMS Israel (3.78 percent); and FMS Japan (3.05 percent) funding in the amount of $7,687,490 will be obligated at the time of award. Funds will expire at the end of the fiscal year. One source was solicited for this non-competitive requirement and one offer was received in response to the solicitation. Naval Supply Systems Command Weapon Systems Support in Mechanicsburg, Pennsylvania, is the contracting activity.
Raytheon Co. Missile Systems, Tucson, Arizona, has been awarded a $93,000,000 indefinite-delivery/indefinite-quantity contract, for Small Diameter Bomb II (SDB II) F/A-18E/F integration. This contract provides for the testing, analysis, support and sustainment of SDB II weapon onto the F/A-18E/F platform with developmental and operational testing. Work will be performed in Tucson, Arizona, and is expected to be completed by July 1, 2023. No funds are being obligated at the time of award. This award is the result of a sole-source acquisition. Air Force Life Cycle Management Center, Eglin Air Force Base, Florida, is the contracting activity (FA8672-18-D-0011).
Lockheed Martin Space, Sunnyvale, California, has been awarded a $48,647,969 modification (P00737) to contract F04701-02-C-0002 for Advanced Extremely High Frequency (AEHF) Satellite Vehicle 1-4. The contract modification is for system-capability augmentation to provide mission-planning functionality to support the AEHF extended data rate transition. Work will be performed in Sunnyvale, California, and is expected to be completed by June 30, 2020. Fiscal 2018 research, development, test and evaluation funds in the amount of $10,215,360 are being obligated at the time of award. Space and Missile Systems Center, Los Angeles Air Force Base, California, is the contracting activity. Total cumulative face value of the contract is $9,151,451,549.
Global Aviation Technologies LLC, Wichita, Kansas, has been awarded a $35,000,000 multiple-award indefinite-quantity/indefinite-delivery contract, for F-16 harness kits and parts. Work will be performed at Global Aviation Technologies LLC in Wichita, Kansas, and is expected to be completed June 27, 2025. National Guard and Reserve Equipment Appropriation funds in the amount of $200 is being obligated at the time of award. This award is the result of a competitive acquisition. Hill Air Force Base, Utah, is the contracting activity (FA8232-18-D-0005, FA8232-18-F-0127).
Interconnect Wiring Harnesses Inc., Fort Worth, Texas, has been awarded a $35,000,000 multiple-award indefinite-quantity/indefinite-delivery contract, for F-16 harness kits and parts. Work will be performed at Interconnect Wiring Harnesses Inc., in Fort Worth, Texas, and is expected to be completed June 27, 2025. National Guard and Reserve Equipment Appropriation funds in the amount of $200 is being obligated at the time of award. This award is the result of a competitive acquisition. Hill Air Force Base, Utah, is the contracting activity (FA8232-18-D-0006, FA8232-18-F-0128).
Richard Manufacturing Co., Ogden, Utah, has been awarded a $35,000,000 multiple-award indefinite-quantity/indefinite-delivery contract, for F-16 harness kits and parts. Work will be performed at Richard Manufacturing Co. in Ogden, Utah, and is expected to be completed June 27, 2025. National Guard and Reserve Equipment Appropriation funds in the amount of $132,247 is being obligated at the time of award. This award is the result of a competitive acquisition. Hill Air Force Base, Utah, is the contracting activity (FA8232-18-D-0007, FA8232-18-F-0124).
Cherokee Nation Aerospace and Defense LLC, Stilwell, Oklahoma, has been awarded a $35,000,000 multiple-award indefinite-quantity/indefinite-delivery contract, for F-16 harness kits and parts. Work will be performed at Cherokee Nation Aerospace and Defense LLC, in Stilwell, Oklahoma, and is expected to be completed June 27, 2025. National Guard and Reserve Equipment Appropriation funds in the amount of $200 is being obligated at the time of award. This award is the result of a competitive acquisition. Hill Air Force Base, Utah, is the contracting activity (FA8232-18-D-0004, FA8232-18-F 0126).
Borsight Inc., Ogden, Utah, has been awarded a $35,000,000 multiple-award indefinite-quantity/indefinite-delivery contract, for F-16 harness kits and parts. Work will be performed at Borsight Inc. in Ogden, Utah, and is expected to be completed June 27, 2025. National Guard and Reserve Equipment Appropriation funds in the amount of $200 is being obligated at the time of award. This award is the result of a competitive acquisition. Hill Air Force Base, Utah, is the contracting activity (FA8232-18-D-0003, FA8232-18-F-0125).
Harris Corp., Colorado Springs, Colorado, has been awarded a $9,198,600 modification (P00877) to contract F19628-02-C-0010 for the National Space Defense Center sustainment effort. Work will be performed at Schriever Air Force Base in Colorado Springs, Colorado, and is expected to be completed by June 29, 2019. Fiscal 2018 operations and maintenance funds in the amount of $9,198,600 are being obligated at the time of award. The Space and Missile Systems Center, Peterson Air Force Base, Colorado, is the contracting activity.
Goodwill Services Inc.,* Richmond, Virginia, has been awarded a maximum $10,350,000 fixed-price contract for base supply and pharmacy system services. This is a one-year base contract with two one-year option periods. Maximum dollar amount is for the life of the contract, including options. Location of performance is Virginia, with a June 30, 2021, performance completion date. Using customer is Defense Logistics Agency Aviation. Type of appropriation is fiscal 2018 through 2020 defense working capital funds. The contracting activity is the Defense Logistics Agency Contracting Services Office, Richmond, Virginia (SP4703-18-C-0509).
Sprint Federal Operations LLC, Reston, Virginia, was awarded a firm-fixed price contract modification for the Defense Information Systems Network European Optical Network Enhancement at Royal Air Force Lakenheath and Link 102 on contract HC1047-15-C-4000. The face value of this action is $7,085,472, funded by fiscal 2018 defense working capital funds. The total cumulative face value of the contract is $215,700,000. Performance will be at various locations within Europe. This modification and the original solicitation were issued on the basis of other than full and open competition, pursuant to 10 U.S. Code 2304(c)(1), only one responsible source and no other type of supplies or services would satisfy agency requirements. The period of performance is a one year base period with nine one-year option periods. The contract is in Option Period Three, Oct. 1, 2017- Sept. 30, 2018. The Defense Information Technology Contracting Organization, Scott Air Force Base, Illinois, is the contracting activity (HC104715C4000P00023).


In UNIX and BSD systems you might not have tac, you can try the less intuitive tail -r instead.
Recursively remove all empty sub-directories from a directory tree using just find. No need for tac (-depth does that), no need for xargs as the directory contents changes on each call to rmdir. We're not reliant on the rmdir command deleting just empty dirs, -empty does that.
Will make many calls to rmdir without using xargs, which bunches commands into one argument string, which is normally useful, but -empty /could/ end up being more efficient since only empty dirs will be passed to rmdir, so possibly fewer executions in most cases (searching / for example).


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Black Host, Nude Model 18+ Soundboard Recommended Image
When: Fri., April 24, 8:30 p.m. 2015
Courtesy Northern Spy Records Black Host
Detroit native Gerald Cleaver has long been one of the most resourceful and creative drummers in the New York jazz scene, shifting between playing straight-ahead sounds as part of trumpeter Jeremy Pelt's quintet and executing mercurial improvisations with pianist Craig Taborn and bassist William Parker in the protean trio Farmers by Nature. But the group that's made it most difficult to pin down his aesthetic has been his Black Host quintet—a fantastic postfusion combo that plays with piquant lyricism, rhythmic elasticity, ferocious power, and a rich timbre. Joined by a group of top-tier collaborators in saxophonist Darius Jones, pianist Cooper-Moore, electric guitarist Brandon Seabrook, and bassist Pascal Niggenkemper, Cleaver directs his own high-octane compositions, a trademark of which is their blend of elegant grace and seething fury. Most of the pieces on the group's 2013 debut, Life in the Sugar Candle Mines (Northern Spy), include his routine layering of slow-moving melody lines over frenetic rhythms—but they can also be impatient, with constant shifts in tempo, energy, and feel. "Ayler Children" opens with a brisk swing: Cooper-Moore plays splashy free-jazz lines and creates a context for the delicate unison between Jones and Seabrook, both of whom eventually dissect the flow, first via Seabrook's nimble picking of the guitar—his sound sits somewhere between instrumental surf and prog metal—and later with a fiery, gut-punching saxophone solo from Jones. The following piece, "Citizen Rose," is a moody, viscous ballad that channels serious turbulence even at lower volume and a slower pace. I can't wait to hear how the music and the band's rapport have developed since the record was made. —Peter Margasak
3111 N. Western Ave. (Roscoe Village)
Theater Music venue Gallery


Robert L. DuPont, director of the National Institute on Drug Abuse (NIDA), made headlines recently when he became one of the first Administration officials publicly to recommend a liberalization of marihuana laws. The occasion was a press conference accompanying the release of Marihuana and Health, NIDA's fifth annual report to the Congress on marihuana research. Recently, Science talked with DuPont and asked him to elaborate on those views.
DuPont, a 40-year-old Harvard M.D., served as Director of the District of Columbia's Narcotics Treatment Administration from 1970 to 1973, where he conducted a comprehensive program for treatment of heroin addiction. In June 1973, Richard Nixon appointed him director of the White House Special Action Office for Drug Abuse Prevention. He held that position until the office was terminated on 30 June 1975. He has been director of NIDA since September 1973.


Ibiza has this apartment complex in Playa d'en Bossa, recently refurbished. The apartments consist of a living room with dining table and kitchenette with microwave, two bedrooms and two bathrooms, allowing up to four people to be accommodated. The accommodations also feature a balcony with a wonderful sea view. In addition, the building has a swimming pool. The nearest attractions are within walking distance of the building and are Ushuaia and Bora Bora Beach Club.


Dawn is over here doing her thing, blogging with a collective of mothers, thinking through and reflecting upon the mixed and wonderful life that is theirs and ours. Here's her latest post, emerging out of both our stubborn insistence to learn how to see.
I gotta give it to Alicia Keys. It takes character to decide to ditch make up in an industry as shallow as the music and television industry. Keys has essentially kicked off another wave of media authenticity with the #NoMakeUpMovement (Jamie Lee Curtis shook the industry with her exposition of photoshopping among celebrity images). Now that another form of natural beauty is trending these days with Alicia Keys, Sanaa Lathan, Kendall Jenner, and others who have committed to natural looks in their public lives, it will be interesting to see if the movement will go beyond trend and revolutionize how we understand beauty as a culture.


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Q: Tracking Admob fill rate in Ionic 2 app I am using the floatinghotpot/cordova-admob-pro plugin to display interstitial ads in my ionic v2 mobile app.
The app functions in such a way that an interstitial ad is displayed after the user completes action. The app is working fine and I have been getting some feedback from my users saying that they don't always see the ad displayed when they complete the action.
Is there a way that I can track the fill rate that I'm getting?


Showing results for tags 'pgatour'.
Shoot Even Par for the Season On the PGA Tour..Where Would You Rank?
A buddy of mine is a former PGA Tour Caddie and current Sport Writer. He and some other caddies started this site that has a lot of great content. The Caddie Network, a lot of inside info from caddies that you may find interesting. Here's one piece that I thought was particularly interesting. https://www.thecaddienetwork.com/what-was-even-par-worth-on-the-pga-tour-in-the-2017-18-regular-season-for-player-and-caddie/ This is a fun read, that if a player shot even par on the tournaments he was qualified to enter for a full season, where do you think he'd finish on the money list. It'd be interesting to see everyone post their guess before reading the article.
New to blog forums, so I look forward to any tips/coaching. Lookng for ways to introduce our Pro-Am tournaments, which bring the Next Generation of Fantasy Golf to golfers at 11,800 courses across the country.


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Q: SQL DENSE_RANK not suitable because of existing table- how to get min/max dates in sequence when val changes I have an existing @table
ID  Date    Val
1   2014-10-01  1
2   2014-10-02  1
3   2014-10-03  1
4   2014-10-04  1
5   2014-10-05  1
6   2014-10-06  1
7   2014-10-07  1
8   2014-10-08  1
9   2014-10-09  1

The Date sequence is of importance.
I need to see the first and last date for each Val sequence:
Select Val,MIN([Date]) as A, MAX([Date]) as B
        from @T
        Group by Val

   Val  From        To
    1   2014-10-01  2014-10-09

The Val column now changes for 3 of these entries:
Update @T set Val = 2 where [ID] between 3 and 5

and returns:
ID  Date    Val
1   2014-10-01  1
2   2014-10-02  1
3   2014-10-03  2
4   2014-10-04  2
5   2014-10-05  2
6   2014-10-06  1
7   2014-10-07  1
8   2014-10-08  1
9   2014-10-09  1

How do I get SQL to return the min/max dates per sequence?
I need to show :
i.e.
1   2014-10-01  2014-10-02
2   2014-10-03  2014-10-05
1   2014-10-06  2014-10-09

If I run the normal Min/Max query, I get
1   2014-10-01  2014-10-09
2   2014-10-03  2014-10-05

Which does not show me that the val was 1 for 1st period,2 for 2nd period
and again 1 for 3rd period
declare @T table(ID int,[Date] date,Val int)
Insert Into @T(ID,[Date],Val)
 values(1,'2014/10/01', 1),
(2,'2014/10/02',    1),
(3,'2014/10/03',    1),
(4,'2014/10/04',    1),
(5,'2014/10/05',    1),
(6,'2014/10/06',    1),
(7,'2014/10/07',    1),
(8,'2014/10/08',    1),
(9,'2014/10/09',    1)

A: Try this
SELECT Val,Min(Date) Min_Date,Max(Date) Max_Date
FROM
(
SELECT ID,Date,Val,SUM(NewVal) OVER (order by ID) AS NewVal
FROM
    (
    SELECT ID,Date,Val,CASE WHEN Val<>LAG(Val, 1) OVER (ORDER BY ID) THEN 1 ELSE 0 END NewVal
    FROM @T
    ) I
) O
GROUP BY NewVal,Val
ORDER BY Min_Date

I adopted the answer from a previous answer to one of my own questions https://stackoverflow.com/a/21635529/1181412
Basically you're using the LAG function to compare the value of the previous row. When it's different you make it a 1, otherwise you use 0. Then you wrap that in a running sum which only increments every time NewVal goes up by 1. The result of the query matches what you're looking for.
The order of the records is obviously very important to this answer. So depending on your specific needs you may need to adjust the OVER clauses.
Edit
Per the comments this is an alternative answer which doesn't use LAG so it works in SQL Server 2008.
SELECT Val,Min(Date) Min_Date,Max(Date) Max_Date
FROM
(
SELECT ID,Date,Val,SUM(NewVal) OVER (order by ID) AS NewVal
FROM
    (
    SELECT M.ID,M.Date,M.Val,CASE WHEN M.Val<>L.Val THEN 1 ELSE 0 END NewVal
    FROM @T M
    LEFT JOIN
        (
        SELECT ID,Date,Val,ROW_NUMBER() OVER(order by ID)+1 NewRowId
        FROM @T
        ) L ON M.ID=L.NewRowId
    ) I
) O
GROUP BY NewVal,Val
ORDER BY Min_Date