ElectroBraid® 1,000 Foot Reel Electric Fencing Line ElectroBraid® is a permanent electric fence line designed especially for horses. It serves as a physical barrier and as a psychological deterrent. It keeps horses away from fencing, prevents them from leaning on it and chewing on it. You can install ElectroBraid® with wood fence posts or T-posts, or as a complement to vinyl fences. ElectroBraid® is SAFE, SECURE and SIMPLE.
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Create an effective, attractive and easy-to-maintain fence by attaching 3 or 4 strands of ElectroBraid® to fence posts spaced 30 to 50 feet apart (compared to conventional horse fences like wire which require a post every 8 or 10 feet). Fence posts can be wood, vinyl or steel, and ElectroBraid® is available in white, black or black/white checkered.
Q&A ElectroBraid® Zareba® and ElectoBraid® answer common questions in its Q&A section to help shoppers with their buying experience. Here's just one question.
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ElectroBraid®'s Answer: Mount ElectroBraid® as a single strand on top of almost any fence. The psychological deterrence to horses is dramatic. Dell Hendricks, an NHRA Reining Champion, had a stallion that regularly jumped his pipe and cable fence to impregnate a neighbor's mares. When a single strand of ElectroBraid® was added, the stallion never jumped the fence again.
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Learn More About ElectroBraid® There's a lot that goes into installing and maintaining an electric fencing system. Fortunately, we have a wide variety of helpful articles to guide you in your efforts as well as keeping your horses happy and healthy. Check out some of these relevant resources to learn more!
Outstanding product! Highly recommend. We have had electrobraid for 10 years and never had to repair it and it doesn't sag. My horse was being chased and ran into the fence and he bounced off of it. No injuries. We are going to be buying more of this product for our new farm.
we have had this for about 2 years. we had a straight line wind event drop 4 trees right on the line, it broke the insulators but the line was perfectly intact. if we had wood fencing it would have been obliterated. we reset the fence and it works just as before. also its easy to install once you get the posts in the ground. I bought extra just for temporary fencing too. great product and it looks better than any other electric fence I have seen. its clear looking and the horses respect it (get the right charger and ground rods). 4 out of 5, the only thing I would change is that it does require retightening especially as the weather (temperature) shifts.
I installed this on 25+ acres of horse farm. Had our first horse kick at the fence yesterday getting his leg behind one wire. Fence is installed exactly as it should be and the roller did not break causing sever injuries to the lower leg. Horse might not recover. Would not suggest this fence to anyone! Most hot wire or tape would have broke but this did not. It stretched out and pulled off 6 line post insulators but didn't break causing the rope to slice right into the tendons on the front of the hock. Please don't fall for the safety gimic, go with wood. I wish I could add a picture but if you've seen a horse get a hind leg caught in wire this is similar.
We are very sorry to hear of this experience and would like to learn more about what occurred. For further assistance, please contact us directly. Our Consumer Relations Team can be reached at 1-888-430-3330.
We have used Electrobraid for over 15 years - and can recommend it - IF I ever have board fence again, it will have electrobraid on the inside to keep the chewers away from it!
We've had our fence for about 2 years. The fence very resilient to limbs that fall on it, no repairs involved, only cut the fallen limbs and it goes right back to it's original position. The horses never get into it, after their initial contact with it. We love this fence.
Q.I found an old reel in the barn that is dirty but should work fine. Is there any way to clean it?
To clean the braid, it can be soaked in mild dish detergent and water. This should be done while the braid is not connected to a charger.
Q.Which color holds up better to the UV the black electro Braid ? or the white? or the black/white?
All of the ElectroBraid® is made from UV resistant materials; one color is not going to be more UV resistant than another.
Q.What is the resistance (ohms/mile) of ElectroBraid?
ElectroBraid® has 12 ohms of resistance for every 1000 ft.


text:
Q: How to make my project URL in github look like this? I am new at github and I developed an application and I want to upload it to github and I am required to make the app accessible on a URL of the type :
http://githubusername.github.io/projectname/#/myapptitle

when I upload files on a new repository with the projectname I don't get the same structure as above. Please help I need to submit my project. Thank you.

A: Have look a github pages right here https://pages.github.com/. There is a very short step by step guide. Basically your repository has to be called: "githubusername.github.io"

redpajama_set_name: RedPajamaStackExchange


text:
\section{Introduction}

Of the $\sim$3,700 exoplanets discovered to date, $\sim$2,900 of them are known to transit their host star.  The vast majority of known transiting planets have come from two types of surveys.  The space-based missions CoRoT \citep{Auvergne:2009}, Kepler \citep{Borucki:2010,Koch:2010}, and the reborn K2 mission \citep[]{Howell:2014}, have discovered nearly 2,600 transiting planets, representing 90\% of all known such planets.  The other main source of known transiting planets are the ground-based transit surveys that use relatively wide field telescopes such as SuperWASP \citep{Street:2003}, HATNet \citep{Bakos:2004}, HATSouth \citep{Bakos:2013}, KELT \citep{Pepper:2007,Pepper:2012}, XO \citep{McCullough:2005}, TrES \citep{Alonso:2004}, and QES \citep{Alsubai:2013}.

Discovering large numbers of exoplanets can reveal the underlying demographics and frequencies of various types of planets \citep{Mayor:2011,Howard:2012}, and for more recent analysis see \citet{(CKS_III)Fulton:2017, (CKS_II)Johnson:2017,  (CKS_I)Petigura:2017, (CKS_IV)Petigura:2017, (CKS_V)Weiss:2017}.  Transiting planets are especially valuable because the transit itself constrains the planet radius and orbital inclination, and together with radial velocity observations, it provides the mass and density of the planet.  Furthermore, for transiting planets it is possible to study the atmosphere of the planet via transmission or emission spectroscopy \citep[]{Charbonneau:2002,Charbonneau:2005,Deming:2005} and constrain the planet's eccentricity with secondary eclipses.  However, those atmospheric observations generally require bright host stars to provide the needed signal-to-noise ratio for spectroscopic observations and thus radial velocity confirmation and mass measurements.

The bulk of known transiting planets come from Kepler and K2, and most of those orbit faint host stars. Of the 1776 transiting planet host stars with a known optical magnitude discovered by the space missions Kepler, K2, or CoRoT, only 85 have an optical magnitude brighter than $V<12$, and only 9 are brighter than $V<10$\footnote{https://exoplanetarchive.ipac.caltech.edu/}.  The ground-based surveys are generally sensitive to brighter host stars; 125 of the 224 host stars of planets discovered by those surveys are brighter than $V\sim 12$, and 23 are brighter than $V\sim 10$.  However, most of the planets discovered by the ground-based surveys are in very short-period orbits, with none of the ground-based discoveries having orbital periods longer than 20 days. Figure \ref{fig:period-mag} shows that only 12 known transiting planets have host stars brighter than $V\sim 10$ and also have orbital period longer than 20 days. This is due to a well-known selection effect against longer period planets in transit surveys \citep[e.g.][]{Pepper:2003,Gaudi:2005}. Since atmospheric studies of planets benefit from being able to probe a range of planetary equilibrium temperatures, this region of parameter space (planets on long periods orbiting bright host stars) must be populated with new discoveries before a more comprehensive study of exoplanet atmospheres can be undertaken.

\begin{figure}[t]
\begin{center}
\makebox[\textwidth][c]{\includegraphics[width=1.0\textwidth]{p_mag.png}}
\caption{Optical magnitude versus orbital period of host stars of known transiting exoplanets. The region inside the red dashed lines shows the 12 exoplanets with bright hosts and orbital periods longer than 20 days.  The data displayed here comes from the NASA Exoplanet Archive, accessed on May 15, 2018.}
\label{fig:period-mag}
\end{center}
\end{figure}

The Transiting Exoplanet Survey Satellite (TESS) is designed to detect transiting planets of bright stars across the whole sky.  However, most of the TESS transit detections will have short orbital periods, due to the short TESS observing time for most of the sky ($\sim27$ days).  In this paper, we explore the potential of combining data from an existing ground-based survey (specifically, the Kilodegree Extremely Little Transit [KELT] survey) with TESS observations.  The goal is to refine the orbital properties of the long-period transiting exoplanets orbiting bright hosts discovered by TESS, which will be extremely valuable for the ability to probe transiting planets at a range of equilibrium temperatures.  We test the feasibility of this endeavor by simulating single transit events as detected by TESS, and then inserting them as periodic signals into real KELT light curves.  We then use standard techniques to recover those signals from the KELT data, and characterize how the recovery rate depends on the properties of the simulated planets and stars.  The approach is effectively ``precovery" of TESS-detected signals from existing data, in which we leverage the information provided by the TESS single transit detections as constraints on the automated search for transits in the existing ground-based survey data.

One of the key goals of TESS is to discover transiting planets orbiting bright stars to provide a rich set of targets for detailed atmospheric measurements by HST and JWST.  Spectroscopic observations can reveal a planet's atmospheric composition, structure, and dynamics, and is a key objective of JWST \citep[]{Beichman:2014}. Atmospheric observations using transmission or emission spectroscopy, verification of planet eccentricity and albedo through secondary eclipse observations, spin-orbit alignment measurements, and transit timing observations all require the ability to schedule observations at future transit times.  Given the high demand for space telescope time, transit observations must be known to a precision of roughly 30 minutes, otherwise precious observing time on high-demand telescopes will potentially be wasted.

It is already known that the ephemerides of even multiple-observed transits degrade over time, and any improvement offered by archival data can save such systems for future space-based transit observation.  \citet{Benneke:2017} demonstrated that this kind of ephemeris improvement was necessary for a 33-day period candidate (K2-18b) observed in the 80-day {\it K2} observing window (see also \citet{Steffanson:2018} for more examples).

In this paper, we explicitly do not attempt to model or predict the number of single-transit detections that TESS will make (see \citet{Villanueva:2018} for such predictions), nor the number of those that the KELT data will be able to precover.  Rather, what we investigate here is the overall efficiency of the precovery procedure to establish the ephemerides of single-transit systems across a range of empirical properties, regardless of the abundance of such systems that are actually seen by TESS.

We discuss the nature of the data used to conduct this analysis in Section \ref{sec:data}, including a description of why the KELT survey is specifically useful for this project. Section \ref{sec:methods} describes the methodology for inserting transits and recovering the signals. Section \ref{sec:results} presents the  results of the recovery tests, describing the types of transiting planets for which this method can be successfully applied.  In Section \ref{sec:disc} we discuss the significance of our findings and ways to build upon these initial results.

\section{Data}
\label{sec:data}

\subsection{The TESS mission}

TESS \citep{Ricker:2015} is a NASA mission that will monitor bright and nearby stars for transiting planets, with a prime mission lasting two years.  The combined field of view is $24^{\circ} \times 96^{\circ}$ with four 4096$\times$4096 pixel CCDs, at $\sim$21\arcsec\ per pixel, and a bandpass between 600 nm and 1000 nm, referred to as $T$-band.  It will acquire observations in two modes.  A selection of about 200,000 stars will be observed at a 2-minute cadence, while all stars in the field of view will be observed at a 30-minute cadence, including about 30 million stars brighter than $T=15$.  The short-cadence observations are commonly referred to as the postage-stamp targets, while the longer cadence observations are referred to as Full Frame Image (FFI) targets.

The 2-min TESS targets are selected based on the suitability for detection of small transiting planets.  That requirement leads generally to a selection of bright, cool, dwarf stars.  The target selection process must account for a number of factors, and can lead to a range of expected planet yields.  Papers that have looked at the expected yields include \citet{Sullivan:2015}, \citet{Bouma:2017}, and \citet{Barclay:2018}.  Each of these papers simulates the TESS survey, and the resulting physical and observational properties of the detected planets.  They find that while the key goals of TESS generally center on small planet discovery, TESS will also discover hundreds of planets larger than 4$R_{\Earth}$ from the 2-minute observations, and of order thousands such planets from the FFIs, with rough agreement between those two predictions about the numbers of planets that will be detected of different sizes.

TESS will observe the sky in a set of pointed observations in which the spacecraft will nearly continuously observe a section of the sky stretching from the ecliptic to the ecliptic pole for 27 days, with each section referred to as a sector.  The mission will step around ecliptic longitude over the course of 13 sectors to cover most of an ecliptic hemisphere over the course of a year, and then rotate and observe the other hemisphere.  Near the ecliptic poles, subsequent sectors will overlap, so that stars in those regions can be observed for many months.  However, the majority of the sky observed by TESS (74\%) will have an observational baseline of only $\sim$27 days. For those transiting exoplanets that have orbital periods longer than 13.5 days, TESS can only capture one or two transits, and for periods longer than 27 days, TESS can only capture one transit. In these cases, the true ephemerides of the planets will be difficult to determine from TESS data alone.

\citet{Sullivan:2015} predict that long period planets (P$>$20d) will account for approximately 20\% of the TESS transit detections, while \citet{Bouma:2017} find similar expectations. Since follow-up confirmation observations are expensive in time and resources, the ability to determine the precise ephemerides for these systems is extremely valuable. Even though the orbital period can be roughly estimated from a single transit \citep{Seager:2003,Yee:2008,Osborn:2016}, additional information is still needed to precisely determine these ephemerides and reduce the associated uncertainty in the transit time.  These estimates require an assumption or constraint on the orbital eccentricity, as well as a precise estimate of the density of the host star, and are often fairly imprecise, thereby necessitating either extensive photometric follow-up, or radial velocity observations \citep{Yee:2008}.

\citet{Villanueva:2018} have done a comprehensive simulation and investigation into the likely TESS single-transit population.  They predict about 1200 single-transit events in TESS.  Those numbers are higher than that of the other simulation efforts by factors of 20\% to 50\%, but possibly because the other simulations are not as complete at the long-period end.  The actual number of single-transit detection will depend on many observational factors unknown at the present, but all indications are that there will a minimum of several hundred such cases.

\subsection{The KELT survey}

The Kilodegree Extremely Little Telescope (KELT) transit survey \citep{Pepper:2007,Pepper:2012} is a photometric survey using two small-aperture (42 mm), wide field ($26^{\circ} \times 26^{\circ}$) telescopes located at Winer Observatory in Arizona, US, (KELT-North) and the SAAO observing station in Sutherland, South Africa, (KELT-South). Each camera contains a CCD with 4096$\times$4096 pixels and provide a pixel scale of roughly 23\arcsec\ pixel$^{-1}$. The effective passband that KELT uses is roughly equivalent to a broad $R$-band filter. The KELT fields cover about 70\% of the sky including a very large fraction of the TESS footprint in both year 1 and year 2 of the TESS mission.  Figure \ref{fig:fields} shows a map of KELT fields, along with Kepler and K2 fields, and a sample set of TESS fields.  Table \ref{tab:typ} lists the names of KELT fields with the sky coordinates of the field centers. Fields are observed every season since their first observation, with observations starting between 2005 and 2013.  Although some fields have been observed for over twelve years, the reduced data available for the analysis in this paper only contained observations for the first eight years of the survey, which sets the maximum time baseline used in the analysis here.  The observing procedure leads to an average cadence of about 20 minutes, with $\sim$1500 observations every year.  All KELT fields overlap at least partially with TESS fields. The photometric precision of KELT ranges from several mmag RMS at the bright end of its magnitude range, around $V=7.5$, where stars begin to saturate in normal KELT observations, to $\sim$5\% RMS around $V=13$. The KELT survey is optimized for the discovery of transiting planets in the range $8<V<10$, and to date has discovered 23 exoplanets (see \citet{Pepper:2018} for references).

\begin{figure}[t]
\begin{center}
\includegraphics[width=1.0\textwidth]{KELT_MAP.png}
\caption{Equatorial map of the sky, with the galactic plane displayed in pink. Colors indicate the locations of the KELT fields (green), the Kepler and K2 fields (cyan), and a sample location layout for the TESS fields (blue).}
\label{fig:fields}
\end{center}
\end{figure}

KELT has several features which make it especially useful for combination with TESS.  The magnitude range of greatest photometric sensitivity overlaps with that of TESS.  The wide field of KELT ($26^{\circ} \times 26^{\circ}$) allows it to cover a large fraction of the entire sky, and the relatively stable and regular observing strategy provides light curves with consistent noise and sampling properties over long time baselines.

\begin{deluxetable}{ccc|ccc|ccc}

\tablecaption{KELT field locations (J2000.0)}
\label{tab:typ}
\tablehead{\colhead{Field} & \colhead{RA (deg)} & \colhead{DEC (deg)} & \colhead{Field} & \colhead{RA (deg)} & \colhead{DEC (deg)} & \colhead{Field} & \colhead{RA (deg)} & \colhead{DEC (deg)}}
\startdata
        N01  &  001.50  & 31.67 & N21  &  200.80  & 57.00 & S19  & 046.00  & -53.00 \\
        N02  &  030.52  & 31.67 & N22  &  240.80  & 57.00 & S20  & 069.00  & -53.00 \\
        N03  &  059.54  & 31.67 & N23  &  280.80  & 57.00 & S21  & 091.80  & -53.00 \\
        N04  &  088.56  & 31.67 & N24  &  320.80  & 57.00 & S22  & 138.00  & -20.00 \\
        N05  &  117.58  & 31.67 & N25  &  054.09  & 79.00 & S23  & 161.00  & -20.00 \\
        N06  &  146.60  & 31.67 & N26  &  126.46  & 79.00 & S24  & 184.00  & -30.00 \\
        N07  &  175.62  & 31.67 & N27  &  197.61  & 79.00 & S25  & 207.00  & -30.00 \\
        N08  &  204.64  & 31.67 & N28  &  269.76  & 79.00 & S26  & 230.00  & -20.00 \\
        N09  &  233.66  & 31.67 & N29  &  342.12  & 79.00 & S27  & 299.00  & -53.00 \\
        N10  &  262.68  & 31.67 & S05  &  091.80  & 03.00 & S28  & 322.00  & -53.00 \\
        N11  &  291.70  & 31.67 & S06/N14  & 114.90  & 03.00 & S29  & 345.00  & -53.00 \\
        N12  &  320.72  & 31.67 & S12/N15  & 253.00  & 03.00 & S30  & 045.00  & -36.00 \\
        N13  &  349.74  & 31.67 & S13  & 276.00  & 03.00 & S35  & 115.05  & -20.00 \\
        N16  &  000.80  & 57.00 & S14  & 299.00  & 03.00 & S36  & 261.00  & -53.00 \\
        N17  &  040.80  & 57.00 & S15  & 322.00  & 03.00 & S37  & 226.80  & -53.00 \\
        N18  &  080.80  & 57.00 & S16  & 345.00  & 03.00 & S38  & 192.60  & -53.00 \\
        N19  &  120.80  & 57.00 & S17  & 000.00  & -53.00 & S39  & 158.40  & -53.00 \\
        N20  &  160.80  & 57.00 & S18  & 023.00  & -53.00 &   &   &   \\
\enddata
\end{deluxetable}

\section{Methods}
\label{sec:methods}

\subsection{General Approach}

Although the KELT survey has a lower photometric precision and duty cycle than TESS, the KELT fields cover a large fraction of the TESS footprint in both the first year of TESS observations of the southern ecliptic hemisphere and the second year of TESS observations of the ecliptic north (Figure \ref{fig:fields}), and the KELT light curves have long time baselines. Furthermore, KELT data are essentially uncorrelated on timescales of longer than a few hours.  When phased and binned on 20-hour timescales (the duration of a long-period transiting planet, the RMS of the detrended KELT lightcurves is typically 0.5 mmag. Thus, for single-transit TESS detections with deep enough transits, KELT can detect the signals in phase-folded data, and determine the ephemerides of the TESS single-transit candidates.  Our overall approach is therefore to simulate TESS single-transit detections, insert the transits into a selection of KELT light curves, and attempt to recover the inserted signals using standard techniques.

\subsection{Selection of KELT Light Curves}

In the analysis for this paper, we made use of KELT light curves already obtained for the survey transit search (see \citet{Siverd:2012} and \citep{Kuhn:2016} for details).  Since the reduction and extraction of KELT light curves is a time-intensive process, we did not make use of the entire set of KELT data, but we will use the full KELT data set by the time TESS light curves are publicly released.

KELT uses a German equatorial mount, which requires a "flip" as it tracks stars past the meridian. Thus, the optics and detector are rotated 180 deg with respect to the stars between observations in the Eastern and Western sides of the meridian. As a result of that meridian flip, a given star experiences different detector defects, optical distortions, PSF shape, flat-fielding errors, etc., in each orientation. Those conditions require us to treat observations in the east and west essentially as two separate data sets \citep{Siverd:2012}.  We also use the Trend Filtering Algorithm (TFA) \citep[]{Kovacs:2005} to correct various types of systematic noise.  This results in 4 separate light curves for each KELT star: an uncorrected east version, and uncorrected west version, and a TFA-processed version of each.

We first select high quality KELT light curves, meaning those with relatively low RMS.  In each KELT field, we create a plot of the RMS of each KELT light curve (before and after TFA-processing) versus approximate V-band magnitude, bin the data in magnitude space between $V=9$ and $V=11$, and fit a curve to the 70th percentile of RMS in each bin.  We define the set of light curves below that fitted curve and also below a fixed limit of 30 mmag RMS as the ``high-quality" KELT light curves for that field.  We also require that each light curve must have at least 3000 observations.  This process is carried out separately for all the KELT light curves in each field orientation.

An example of the selection method in one field is shown in Figure \ref{fig:RMS}.  The orange line represents the 30 mmag limit of RMS, while the blue line is fitted to the 70th percentile of the RMS range in each bin. Stars whose light curves (in both raw and detrended version) fall below both the orange and blue lines are selected for analysis.

\begin{figure}[t]
\begin{center}
\makebox[\textwidth][c]{\includegraphics[width=1.0\textwidth]{N05_west_rms_rms.png}}
\caption{RMS vs. approximate V magnitude for raw data in one example field (west field of N05) with selection criteria. The orange dashed line represents the 30 mmag cut; blue dots correspond to the 70th percentile RMS in each 0.25 magnitude bin between V=9 and V=10.25, and the blue solid line represents the fit to the dots.  Stars brighter than $V\sim7.5$ experience saturation and nonlinearity effects, and so have large scatter.}
\label{fig:RMS}
\end{center}
\end{figure}

If both the east and west light curve of a star pass these cuts, then the light curves are combined into a single light curve and used for later steps. However, if the star only passes in east (west) field, then the light curve in only east (west) field is used. In all, $\sim$360,000 stars are selected from the 4.5 million KELT stars with light curves.  The selected stars are then cross-matched with the TESS Candidate Target List \citep[CTL;][]{Stassun:2017}.  The CTL contains stellar information such as TESS mag (T-mag), $T_{eff}$, stellar mass, and radius.

We end up with $\sim$133,000 combined KELT light curves matched to the TESS CTL ($\sim$70,000 light curves in northern KELT fields and $\sim$63,000 light curves in southern KELT fields). In addition, $\sim$52,000 KELT light curves in solely east or west orientations are selected. The fact that less than half the high-quality KELT light curves match to the CTL is not surprising.  The CTL contains only stars that are especially useful for transit detection, meaning that giant stars and very hot stars (OBA spectral types) are generally excluded, while no such restriction was applied to the KELT light curves.

We display distributions of the number of observations and observational time baseline for all KELT light curves that pass these cuts in Figure \ref{fig:hist}.  Because KELT-North has been observing for longer than KELT-South, and generally has more observations and a longer time baseline, we split the two sets of light curves.  For the selected KELT-North light curves, the number of observations is irregularly distributed between 3,000 and 11,000, while the baselines range from 2.5 years up to $\sim$8 years. For the selected KELT-South light curves, the number of observations is irregularly distributed between 3,000 and 8,000, while the baselines range from 2.5 years up to $\sim$6 years. The KELT survey is ongoing, and the number of observations and length of the observing baseline will continue to grow as new observations are made, and as more existing data are reduced.

\begin{figure}[t]
\begin{center}
\makebox[\textwidth][c]{\includegraphics[width=1.2\textwidth]{hist.png}}
\caption{Histogram distributions of the number of data points (left panel) and time baseline (right panel) of matched KELT-North and KELT-South combined light curves used in this analysis.}
\label{fig:hist}
\end{center}
\end{figure}

KELT is a magnitude-limited survey.  As such, it is affected by selection biases including Malmquist bias \citep{Bieryla:2015}.  As a result of that, plus the selection of the brighter, low-RMS light curves, the stars that make it past the cuts tend to be solar mass or greater.  Figure \ref{fig:stellar-overall} illustrates the stellar properties for the matched KELT-North combined light curves.  Most stars are generally F-type, with radii between 1 and 2.5 $R_{\odot}$, masses between 1 and 2 $M_{\odot}$, and effective temperatures between 5500 and 7500 K.  The TESS magnitudes range mostly from $9 < T < 11$.

\begin{figure}[t]
\begin{center}
\makebox[\textwidth][c]{\includegraphics[width=1.2\textwidth]{ALL.png}}
\caption{Histograms of stellar properties (radius, mass, TESS magnitude and effective temperature) for the matched KELT-North combined light curves.}
\label{fig:stellar-overall}
\end{center}
\end{figure}

\subsection{Inserting Simulated Transits}

We assume that the transit depth $\delta$, transit duration $T$, and mid-transit times ($T_C$)
will be easily measurable in TESS data for the events relevant to this work. Since the smallest RMS for the brightest stars in KELT data is a few mmag, we are only considering events detected in TESS with depths of this order and larger. This corresponds very roughly to planetary radii larger than $4 R_{\Earth}$ for planets transiting mid-type main sequence stars.

The following parameters were used to insert box-shaped transits into each selected KELT light curve: The $T_C$ was generated randomly between July 1st, 2018 and July 1st, 2020 corresponding to the expected start and end of the primary TESS mission; the orbital period was assigned randomly from 13.5 days to 300 days in log space ; the transit depth was assigned randomly from 3 mmag to 20 mmag in log space; the transit duration was estimated based on Equation (18) and (19) of \citet*{Winn:2010} by assuming equatorial transits in a circular orbit ($b=0$):
\begin{equation}
\label{eqn:duration}
T = 13\;\mathrm{hr}
\left(\frac{P}{365\;\mathrm{days}}\right)^{1/3}\left(\frac{\rho_{\star}}{\rho_{\odot}}\right)^{-1/3}.
\end{equation}
The stellar density $\rho_{\star}$ in equation (2.1) was calculated from stellar mass and radius obtained from CTL-6.

The particular ranges of transit depth and orbital period we probe here are based on a rough accounting of where the KELT data will be most useful. The single-transit events seen by TESS will generally have minimum orbital periods of half the 27-day observing baseline for a sector, or 13.5 days.  We use 300 days as a convenient outer range for periods to probe, although see the discussion at the end of the paper for comments on that limit. We selected a minimum depth of 3 mmag since that is about the shallowest transit for which a transit can be detected in KELT data, and a maximum depth of 20 mmag since that is approximately the greatest transit depth observed to date, although there are a handful of known transiting planets with larger transit depths. We also reject those inserted light curves ($\sim$15\% of the total sample) whose transit signals correspond to transit planets with radius larger than twice Jupiter's radius.

\iffalse
\begin{figure}[t]
\begin{center}
\makebox[\textwidth][c]{\includegraphics[width=1.2\textwidth]{stellar_Period_Depth.png}}
\caption{Distributions of stellar properties (radius, mass, density, TESS magnitude and effective temperature) in the depth-period grid cells for the matched KELT-North combined light curves.}
\label{fig:stellar-depth-period}
\end{center}
\end{figure}
\fi

Since transit signals are inserted randomly into the light curves, the properties of the host stars are uniform across the range of transit depths and orbital periods.  However, we can use equation \ref{eqn:duration} to relate the inserted orbital periods, along with the stellar densities, to plot the distribution of stellar properties across transit duration in Figure \ref{fig:stellar-depth-duration}.  We see that the distribution of stellar parameters is clearly not uniform across transit duration. Specifically, smaller, higher density, cooler stars exhibit shorter transit durations. Since the transit duration for a given orbital period depends on the mass and radius of the star, signals that were inserted with a given period will have shorter duration for smaller stars.  Long duration transits generally correspond to those with long orbital periods, as in equation \ref{eqn:duration}. But they also scale with the low stellar densities and hence large stellar radii, and are therefore preferentially hotter stars or sub-giants. These features have important implications for the use of this analysis for TESS users, as explained in the discussion below.

\begin{figure}[t]
\begin{center}
\makebox[\textwidth][c]{\includegraphics[width=1.2\textwidth]{stellar_duration.png}}
\caption{Distributions of stellar properties (radius, mass, density and effective temperature) in transit duration parameter space for the matched KELT-North combined light curves, with stellar properties taken from the TIC. The light gray region corresponds to the median absolute deviation in one hour bins.  Note that since the TIC determines stellar mass based on $T_{eff}$ (see section 3.3.2 of \citet{Stassun:2017}), the plot of stellar mass looks almost identical to that of temperature.}
\label{fig:stellar-depth-duration}
\end{center}
\end{figure}

\subsection{Recovery of Inserted Transits}

We use the box-fitting least-squares algorithm (BLS) \citep{Kovacs:2002}, as implemented in the VARTOOLS \citep{Hartman:2016} software package, to search for transits in the KELT data with a fixed transit duration at a given $T_C$, using the values from the inserted signals.  The concept behind this approach is that since the parameters $T_C$ and $T$ for a given transit signal will be known with high fidelity from the TESS observations, we can then search the KELT light curves for repeating transit signals with the same duration and transit time as seen in the TESS data.  While we could also require that the search algorithm require the transit depth to be the same as seen in the TESS data, we believe that such a restriction would not be advisable.  Although KELT and TESS have roughly similar pixel scales, the different bandpasses, field angles, and other properties of the telescopes yield different blending properties for the same stars, and thus different measured transit depths are expected.  We searched for signals with periods ranging from 10 days to 310 days, with a frequency resolution of 300,000.  This period range is similar but not identical to the inserted period range.

\section{Results}
\label{sec:results}

For the bulk of the analysis we present here, we investigate only the collective results using KELT-North lightcurves.  Compared to KELT-South, the KELT-North data cover longer time baselines and have more total observations, and will generally yield larger rates of precovery.  We do that partly to provide an optimistic perspective on the value of this effort for TESS.  Also, since the data available at the time of this analysis does not include the last one to four years of KELT data (still being reduced), the larger current KELT-North data set is a better reflection of the KELT data available for precover in the next year.  For completeness sake, we include summary plots of the KELT-South precovery rates at the end of the paper.

For a successful recovery of an inserted transit signal, we require that the percent error between the output period and the inserted period be within 0.01\%.  That limit was selected because we find it to naturally divide the populations of recovered versus failed cases, as shown in Figure \ref{fig:period_percent}.  The exact value of the cut is somewhat arbitrary, but can be shifted with little overall effect on the overall results.  However, for the frequency spacing used in this analysis (300,000), the cut cannot be much smaller than that, without running into the resolution of the retrieved period at the long-period end.

This criterion cannot be used to determine actual recovery of signals with real data, since it is not an observable, but we can use it to gauge the accuracy of the precovery process for different star, planet, and light curve properties.  To examine the practical use of the precovery approach, we investigate the use of the SNR of the recovered transit below in section \ref{sec:prac}.

As is common in searches for periodic variability, we find that a small number of the searches identify a period that is a small fractional multiple of the true period, at a rate much higher than random chance, but not as high as the true period recovery rate.  Overall, we find that between 1\% and 7\% of the inserted signals are found within 0.01\% of either 1/2, 3/2, or twice the inserted period.  In the analysis below, we do not include those cases as successful recoveries, but we discuss how they might be used in the discussion section.

\begin{figure}[t]
\begin{center}
\makebox[\textwidth][c]{\includegraphics[width=1.0\textwidth]{Period_percent_scatter_hist.png}}
\caption{The histogram and scatter distributions of the fractional period recovery with inserted orbital period for KELT North light curves. The red dashed lines represent 0.01\%.}
\label{fig:period_percent}
\end{center}
\end{figure}

We can examine how well our results match theoretical expectations. The SNR of a transit \citep{Pepper:2003,Gaudi:2005} is:
\begin{equation}
\label{eqn:SNR}
SNR = \sqrt{N f_{tr} }\frac{\delta}{\sigma}
\end{equation}
where $N$ is the total number of data points in light curve, $f_{tr}$ is the fraction of time the planet is in transit ($T/P$), $\delta$ is the transit depth and $\sigma$ is the fractional photometric uncertainty.  We can express SNR in terms of the stellar density and orbital period:
\begin{equation}
\label{eqn:SNR_period}
SNR = \sqrt{N} \frac{\delta}{\sigma} {\left(\frac{3}{G\pi^2}\right)}^{1/6}P^{-1/3}\rho_{\star}^{-1/6}
\end{equation}
We can also express SNR in terms of transit duration:
\begin{equation}
\label{eqn:SNR_duration}
SNR = \sqrt{N} \frac{\delta}{\sigma} {\left(\frac{3}{G\pi^2}\right)}^{1/2}T^{-1}\rho_{\star}^{-1/2}
\end{equation}

From these equations, we can see that the SNR is proportional to the transit depth, while it has negative correlation with stellar density, orbital period, and transit duration.

\subsection{Recovery results}

We display the results of these tests in several ways. The simulated recovery rate distributions across transit depth vs.\ orbital period and transit depth vs.\ transit duration for the KELT-North combined light curves are shown in Figure \ref{fig:north_rate_period} and Figure \ref{fig:north_rate_duration}, respectively.

\begin{figure}[t]
\begin{center}
\makebox[\textwidth][c]{\includegraphics[width=1.0\textwidth]{NC_Depth_Period_Bin10x10.png}}
\caption{Recovery rates of simulated transits for orbital period-transit depth bins of the KELT-North light curves. The grayscale bar indicates the fraction of the transits that are correctly recovered, which is also represented by the percent value in each bin.}
\label{fig:north_rate_period}
\end{center}
\end{figure}

\begin{figure}[t]
\begin{center}
\makebox[\textwidth][c]{\includegraphics[width=1.0\textwidth]{NC_Depth_Dur_Bin10x10.png}}
\caption{Recovery rates of simulated transits for transit duration-transit depth bins KELT-North light curves. The grayscale bar indicates the fraction of the transits that are correctly recovered, which is also represented by the percent value in each bin.}
\label{fig:north_rate_duration}
\end{center}
\end{figure}

In Figure \ref{fig:north_rate_period}, the recovery rates decrease with smaller depths and longer periods monotonically. The inserted transit depths and orbital periods are distributed uniformly across the full set of light curves, and so the number of data points in the light curves, stellar density, and photometric uncertainty, are distributed uniformly across Figure \ref{fig:north_rate_period}.  Therefore from Equation \ref{eqn:SNR_period}, the only parameters that affect the recovery rate difference in this plot are transit depth and orbital period.

In Figure \ref{fig:north_rate_duration}, the recovery rates no longer vary monotonically from upper left to lower right. This is because stellar densities are no longer uniformly distributed across transit duration (see Figure \ref{fig:stellar-depth-duration}), and the stellar density has negative correlation with transit duration (Equation \ref{eqn:duration}).  That is because from Equation \ref{eqn:SNR_duration}, the relation between SNR and transit duration becomes more complex. To examine this effect across transit duration, we divided transit duration into 20 bins. In each bin, we calculated the recovery rate and average SNR, and plot them in the same figure to compare their trend (Figure \ref{fig:snr_rate}). We see that the overall trends are similar in structure.  We can see the reasons for this behavior in Figure \ref{fig:stellar-depth-duration}, which shows that at short transit durations the stars are significantly more dense.  That explains the decrease in recovery at very short transit durations.  Conversely, Equation \ref{eqn:SNR_duration} shows that SNR is a stronger function of transit duration than stellar density.  Therefore at long durations, we see an increase in recovery rates.

\begin{figure}[t]
\begin{center}
\makebox[\textwidth][c]{\includegraphics[width=1.0\textwidth]{rate_snr.png}}
\caption{Recovery rate (red line) and calculated SNR (blue line) versus transit duration.  The effects of populating planets evenly in period space, but then converting to transit duration, created a more complex trend in transit duration when accounting for the underlying stellar population.}
\label{fig:snr_rate}
\end{center}
\end{figure}

The plots convey the operational efficiency of the existing KELT light curves in terms of the key parameters of the inserted signals: transit depth and orbital period or transit duration.  It is also possible to display the vertical axis not in terms of transit depth, but rather in terms of planet radius $r$, which is shown in Figure \ref{fig:north_Rp}.  The planet radius is calculated based on the inserted transit depth and the host star's radius from the CTL, assuming perfect deblending of the host star from any nearby neighbors.  The listed radius is therefore a ``true" depth rather than an ``observed" depth.  Since the simulated transits were drawn from a logarithmic distribution of depths, rather than radii, a small number of light curves are excluded from the plot, in which the inserted signals represent planets smaller than 0.5 $R_J$.  We have also continued to exclude the small number of initially inserted signals that would represent planets larger than 2 $R_J$.

For the KELT-North light curves, for warm Jupiter systems (planet radius of 0.9 to 1.1 $R_J$ and $13.5 < P < 50$ days) we recover 30\% to 50\% of the transits. For warm inflated Jupiter systems (planet radius of 1.1 to 2 $R_J$), we recover 50\% to 80\% of the transits. For temperate Jupiters ($50 < P < 300$ days), we recover 5\% to 18\% of the transits, and for temperate inflated Jupiters, we recover 10\% to 50\%. For warm Saturns (planet radius 0.5 to 0.9 $R_J$ and $13.5 < P < 50$ days) we recover 10\% to 30\% of the transits.

\begin{figure}[t]
\begin{center}
\makebox[\textwidth][c]{\includegraphics[width=1.0\textwidth]{NC_Rp_Bin5x5.png}}
\caption{Recovery rate distributions displayed across period vs.\ planetary radius space (left) and transit duration vs.\ planetary radius space (right) for the KELT-North combined light curves. The color bar indicates the fraction of the transits that are correctly recovered, which is also represented by the percent value in each bin.}
\label{fig:north_Rp}
\end{center}
\end{figure}

\subsection{Precovery in Practice}
\label{sec:prac}

We can display the results of this analysis in a way that would be more useful for investigators pursuing TESS candidate follow-up.  Importantly, the previous plots considered a successful recovery as one in which the strongest peak in the BLS search corresponded to an orbital period within 0.01\% of the true period.  However, no signal strength criterion was applied.  We adopt an approach whereby for each bin in transit depth-transit duration space, we determine the value of the signal-to-pink-noise (SPN) ratio such that at least a given fraction of all the light curves in that bin with that SPN value demonstrate a successfully recovered period.

That information can be seen for the full set of light curves in Figure \ref{fig:SPN_rec}, showing the distribution of SPN values, along with the fraction of light curves for a given SPN for which the signal was successfully recovered.  At SPN$\sim6$, half the signals were recovered, and at SPN$\sim7$, about three fourths were recovered.

\begin{figure}[t]
\begin{center}
\makebox[\textwidth][c]{\includegraphics[width=1.0\textwidth]{SPN_full_log.png}}
\caption{Distribution of SPN values for all light curves, colored by whether the transit signal was recovered with the correct period.  The green color indicates that the recovered period was a low-integer multiple or fraction of the inserted period.  The lower panel indicates the fraction of the light curves at a given SPN value in which the signal was successfully recovered.  At SPN$\sim6$, half the signals were recovered.}
\label{fig:SPN_rec}
\end{center}
\end{figure}

While those fractions provide overall guidance to the SPN threshold to use to determine a likely successful signal detection, it would be more useful to break that number down across the range of observable parameters from the TESS signals.  We therefore compute the distributions from Figure \ref{fig:SPN_rec} across transit depth and transit duration space, and calculate the SPN values for which more than 10\%, 50\% and 90\% of the signals are successfully recovered.

We display the results of that analysis in Figure \ref{fig:spn_north}.  The plot displays the confidence that a user can have regarding the ability of the KELT data to detect the signal.  For each bin, we display the fraction of KELT light curves in the bin such that 90\%, 50\%, and 10\% of the light curves above the corresponding SPN limits are recovered at the correct period.  Those numbers provide guidance for how useful the KELT light curves can be for obtaining ephemerides of single-transit signals, depending on the value of individual planet candidates and the availability of observing resources.

For instance, consider the bin for signals with durations of 8.2 to 11.7 hours and depths of 9 to 14 mmag.  We find that in 29\% of KELT light curves with signals with those properties, the SPN value of the transit search is large enough for a better than 90\% confidence that the BLS search recovers the true period.  In 43\% of light curves, the SPN value is large enough for better than 50\% confidence in the recovery reliability, and in 50\% of light curves, the SPN value is large enough for better than 10\% confidence in the recovery reliability.  The corresponding SPN values for each cut are displayed next to the percentage values.

Someone analyzing a single-transit event in TESS with these characteristics can refer to this figure.  If the target has a high-quality KELT light curve, and the SPN result of a BLS search is greater than the 90\% threshold for that signal, or SPN$=7.8$, they can schedule observations to confirm the ephemeris with a 90\% confidence of a successful detection. If observational resources are plentiful, the observer may be willing to accept a 10\% success rate, and can choose to pursue a large number of targets.

The results described in this section so far make use only of KELT-North data, to demonstrate the potential of this project.  For completeness, we display the plots of recovery rates in Figures \ref{fig:south_rate_period} and \ref{fig:spn_south} below.  We see that the overall patterns are similar to those for KELT-North, only with lower recovery rates to to the smaller number of data points and shorter time baselines.  With the addition of yet-unreduced data for both KELT-North and KELT-South, the recovery rates for both sets should improve significantly. As more data is acquired over the next few years, both the time baseline and number of data points will grow, further improving the recovery rates.

\begin{figure}[t]
\begin{center}
\makebox[\textwidth][c]{\includegraphics[width=1.0\textwidth]{SPN_dur_depth_v4.png}}
\caption{Fractions of KELT-North light curves that pass SPN criteria in transit duration-transit depth bins, and the corresponding SPN values. The percentages reflect the fraction of KELT light curves in that bin such that if the SPN value is greater than the indicated value, there is a 10\%, 50\%, or 90\% confidence that the recovered period is correct, from upper left to lower right in each bin.  The color bar indicates the fraction of KELT light curves that pass the 50\% confidence threshold.}
\label{fig:spn_north}
\end{center}
\end{figure}

Figures \ref{fig:succ_1} through \ref{fig:fail_2} show example light curves where the inserted signal was successfully or unsuccessfully recovered. A transit with a relatively short period of 35 days and shallow depth of 3 mmag was successfully recovered in Figure \ref{fig:succ_1}.  A transit with a long period of 250 days and deeper depth of 7 mmag was successfully recovered in Figure \ref{fig:succ_lp}. An example of a failure to recover is shown in Figure \ref{fig:fail_1}.  In that case, the transit depth of 5 mmag is too shallow compared to the scatter in the KELT data. Figure \ref{fig:fail_2} shows a case where the KELT observations happen to miss the inserted transit completely.

\subsection{Considerations for 2-min Targets vs. FFIs}

The tests described so far do not depend on whether the TESS planet candidates are extracted from the 2-min postage stamps or the 30-min FFIs.  The main difference between the two types of data that we consider here are the longer cadence of the FFIs, which could lead to greater errors in the measured transit duration of the resulting single transits.  We examine that effect by taking a subsample of the successfully recovered light curves and add a random error to the transit duration ranging from -90 to +90 minutes.  Figures \ref{fig:north_durerr} shows the impact of the duration error on the recovery rates for different period and depth regimes in the KELT-North combined data. We find that any uncertainty in the transit time and duration caused by the lower cadence of the 30-minute FFIs causes at most a $\sim$15\% reduction in recovery rates.

\begin{figure}[t]
\begin{center}
\makebox[\textwidth][c]{\includegraphics[width=1.0\textwidth]{NC_durerr_Bin5x5.png}}
\caption{Recovery rate distribution exploring the effect of an error in the identified inserted transit duration.  The plot shows recovery rate for a range of duration error versus orbital period and transit depth for the $\sim$28,000 KELT-North light curves with simulated transits for which the transits were successfully recovered in the previous step.}
\label{fig:north_durerr}
\end{center}
\end{figure}

\section{Discussion}
\label{sec:disc}

Since this work demonstrates that KELT and similar ground-based surveys have the ability to detect significant numbers of long period exoplanets, it is natural to ask why the surveys have not already detected them.  That is, the simulations described in this paper do not use actual TESS light curves, rather just signals inserted into archival KELT lightcurves, so if such signals are already in there, why are they not already found?  In fact, none of the three most productive ground-based transit surveys (WASP, HAT, and KELT) have detected a transiting planet with an orbital period longer than 20 days.

The reason such signals have not been discovered so far is that long-period planets have smaller SNR, especially for transit surveys that search in phase-folded data, along with the fact that at longer periods the transit probability is intrinsically smaller.  Therefore ground-based surveys would have to intensively look for rare, low-SNR signals, which usually means lowering a SNR threshold on an automated search algorithm.  That will result in a large number of spurious false positive candidates, which themselves are more difficult to follow up and confirm for long-period and long-duration signals.  Existing surveys like KELT simply do not have the resources to chase that many candidates.

However, the availability of the TESS signal short-circuits that problem.  Because TESS sees a transit at a particular time, for a particular star, with a particular transit duration, the parameter space that must be searched by an algorithm like BLS shrinks dramatically.  For a given light curve, it is no longer necessary to search through a range of transit phases and transit durations.  Rather, the $T_C$ is known, along with the duration, and the only unknown parameter is the period.  Therefore the SNR threshold is effectively lowered, and smaller signals can be detected since the spurious signal rate is lowered.  Mostly, though, the availability of the TESS signals means that the particular stars with signals are known, shrinking the number of light curves to be searched from hundreds of thousands to hundreds, since only those stars whose light curves that show a signal in TESS need to be searched.  That means that the total number of candidates that emerges from the automated cuts is reduced by several orders of magnitude, and can be followed up with a reasonable set of observing resources.

\subsection{Potential for Improvement}

The procedures outlined here represent a first attempt to quantify the value of ground-based transit surveys for detecting single-transit events in TESS.  There are a number of steps in which we have simplified the analysis, and which can be improved in future work.  Some of those steps involve a more realistic set of planet-star system properties.  Although we are using real KELT light curves and the actual stellar properties for those stars in from the TIC, we have assumed circular and equatorial transits.  A realistic distribution of those parameters would allow for a more accurate set of likely recovery rates.  It would also be useful to redo the analysis using realistic transit models that account for limb-darkening, rather then using box-shaped inserted transits.  In general, we would not expect that difference to have a large effect \citep{Gould:2006}, but it should be investigated especially for stars observed with the 30-minutes cadence by TESS.

Furthermore, the analysis in this paper has addressed the overall sensitivity of the process - we have not attempted to perform an actual simulation of the total numbers of single-transit event TESS will detect, and the resulting total numbers that can be precovered using the KELT data.  We intend to conduct such an exercise, using the \citet{Villanueva:2018} simulations.

A key issue we have not addressed here is the combination of existing ground-based photometry and radial velocity (RV) measurements.  A small fraction (about 5\%) of the cases included in this analysis are systems where the inserted transit signal was found at a fractional multiple of the true period.  Without additional information, those cases do not represent strong opportunities for follow-up, since it would be necessary to conduct several additional observations to investigate each separate multiple of the precovered period. However, if RV observations were available that ruled out one or more of the common multiples, the probability of catching the transit would significantly increase.  In fact, RV observations could enhance the value of photometric precovery overall by constraining the possible orbital periods.  The observational needs for such an effort is described in \citet{Villanueva:2018} and also in Dragomir et al. (in preparation).  The availability of photometric precovery should be a component to such a project, allowing observers to conserve resources by maximizing the probability of ephemeris conformation.

In a similar way, the assumption of a circular or near-circular orbit can be used to estimate the orbital period as outlined by \citet{Yee:2008}.  That information can be used to constrain the precovery results to improve the reliability of the precovery-derived periods at a given SNR, or to increase the number of candidates that can be investigated by selecting a lower SNR cutoff at the same confidence of correct transit recovery.

One final point is that while KELT might be the best-positioned of the current ground-based transit surveys for TESS single-transit precovery, other survey data should also be explored.  The SuperWASP and HatNet surveys should have the ability to conduct a similar sort of precovery, especially for the lower-mass stars to which KELT is less sensitive.  That is especially the case for the recently started Next Generation Transit Survey \citep[NGTS]{Wheatley:2018}, and the Multi-site All-Sky CAmeRA (MASCARA) survey \citep{Talens:2017} should be especially sensitive to transits of very bright ($V<8$) stars.  Combining data for the same star from multiple surveys with complementary time baselines and observing seasons offers an especially rich possibility for transit detection, as noted by \citet{Fleming:2008}.

\subsection{Planet Confirmation}

Precise ephemerides are important for determining the planetary nature of TESS transit candidates, whether via dynamical confirmation or statistical validation \citep{Morton:2012,Torres:2011}.  That is because the TESS pixels are very large on the sky, about 20 arcsec across.  Because of that large pixel scale, a large fraction of TESS transit candidates will be blended with nearby stars in the TESS photometry.  That will create uncertainty about which star is experiencing the transit, diluting the depth of the transit signal itself, and thus affecting the derived planet radius.  Depending on the degree of blending and the depth of the transit, the TESS data, along with high-resolution images of the region around the target, can be used to determine the target star and true transit depth.  But that will not be the case in all circumstances, primarily for crowded regions and shallow transits.  It will therefore be necessary to conduct additional time-series photometry with higher spatial resolution to determine whether the signal is coming from the expected target star or a nearby blended eclipsing binary.  In such circumstances, having a precise ephemeris will allow the efficient planning of observations and conserve observing resources.  Additionally, reliable ephemerides can allow radial-velocity observers to schedule observations at quadrature for efficient dynamical confirmation of planets.

The TESS mission is planning follow-up observations to confirm planet discoveries through the TESS Follow-On Program (TFOP).  TFOP will be focused on confirming the primary targets of the TESS mission, which are small planets with radii smaller than 4 $R_E$.  There is also a project being developed at the NASA Exoplanet Science Institute (NExScI) called ExoFOP-TESS to organize follow-up observations for all other TESS transit candidates, including giant planets and candidates detected in the FFIs.  Given the sensitivity of the KELT photometry, this kind of precovery will be particularly useful for the ExoFOP-TESS project.

\section{Conclusion}

Between the targeted postage stamps and the FFIs, the TESS data will contain tens of thousands of detected transiting exoplanets, amidst hundreds of thousands of false positive signals, most of which will be eclipsing binary stars \citep{Sullivan:2015}.  Having precise and reliable ephemerides for the TESS transit candidates will be crucial for two reasons: planning confirmation observations, and conducting follow-up characterization studies. The recent announcement of the launch delay for JWST until 2021 means that even more time will pass between the TESS observations and JWST atmospheric observations, exacerbating the effects of imprecision of ephemerides as seen by \citet{Benneke:2017}.

This work demonstrates that the use of ground-based photometric data can be used to recover the ephemerides of TESS single transit events.  Specifically, we find that when given information about a single transit from TESS data ($T_C$ and transit duration), the signal of the phase-folded transit can be detected in KELT data, and thus determine the ephemerides, of 30\% to 50\% of warm Jupiters, of 5\% to 18\% of temperate Jupiters, and 10\% to 30\% of warm Saturns and Neptunes.  This technique can likewise be applied to data from other ground-based transit surveys in conjunction with TESS, further increasing the number of single-transit events from TESS with precisely determined ephemerides.

The work described here represents a proof of concept for the approach.  In future papers, we intend to explore how the efficacy of precovery methods like this depends on other system parameters, such as the host star properties.  We will also explore the particular value of this approach in cases where TESS sees two or three transits.  In such cases, the initial ephemerides will be much more constrained by the TESS data directly, and we will examine the marginal increase in precision provided by data from ground-based data, rather than the overall recoverability question we probe in this paper.

\acknowledgments{
ADS, SIMBAD,
This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program.

}

\bibliographystyle{apj}

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A knife-wielding 21-year-old attacked a man on Martense Street on Nov. 25, leaving him with a cut to the chin that needed four stitches to close.
The two men were arguing between Flatbush and Bedford avenues at 11:10 pm when the assailant began swinging his blade above his victim's head.
"Back up or I'll cut you," the assailant threatened.
When the victim didn't do what he was told, the sinister slicer made good on his promise, police were told.


text:
Home / News & Insights / Whistleblower Law Insights / Drug packaging is another way pharmaceutical companies are overcharging
Drug packaging is another way pharmaceutical companies are overcharging
The drug packaging methods of some pharmaceutical companies are forcing insurers, patients, and the government programs like Medicare to pay for unused drugs, according to a recent study. Source: bmj.com
Medicare, patients and private health insurers are wasting billions of dollars a year because of the way drug companies are packaging some of their products.
The waste from could add up to roughly $3 billion in 2016 alone, according to a recent report from BMJ, which was formerly known as the British Medical Journal.
The report details how producers of certain cancer drugs – Amgen, Merck, Genentech, Eli Lilly, and Jazz Pharmaceuticals, to a name a handful – sell their drugs in amounts that are inconsistent with typical dosages.
Take Genentech's Avastin, which is used to treat a variety of cancers. According to the report, the typical dosage for a 70kg (154lb) patient is 350mg. But Genentech only sells Avastin in vial sizes of 100mg and 400mg. That leads to 50mg of waste per patient.
The estimated total cost of the drug packaging waste in 2016 could be $284.5 million, according to the report.
As of now, it's up to the drug companies themselves to fix the drug packaging problem. A Merck spokesperson told Marketplace, a public radio news show, the company is moving to a fixed dose to eliminate waste in their drug, Keytruda.
An Amgen spokesperson expressed a decidedly different attitude, saying the company believes additional vial options are misguided and threaten patient safety, according to Marketplace.
"Drug companies are quietly making billions forcing little old ladies to buy enough medicine to treat football players, and regulators have completely missed it," Peter Bach, director of the Center for Health Policy and Outcomes at Memorial Sloan Kettering and a co-author of the study told the New York Times. "If we're ever going to start saving money in health care, this is an obvious place to cut."
Though the study focuses on pharmaceutical companies that produce expensive cancer drugs, they are not the only ones who employ questionable packaging-related practices, nor is the problem only related to cancer.
In 2013, a company acquired by US Renal Care agreed to pay a $7.3 million settlement for allegedly charging patients for the unused overfill of an anemia drug called Epogen. Amgen, the company that makes Epogen, typically overfills their vials by 11 percent to allow syringes to withdraw the needed amount. Amgen does not charge for this extra 11 percent because it is unusable.
According to a whistleblower lawsuit filed by Phillips & Cohen, Dialysis Corp. of America allegedly billed Medicare for not just the Epogen patients received, but the extra 11% that was thrown away. At one point, Epogen reimbursements accounted for more than 25 percent of DCA's medical-services revenue.
What the drug companies mentioned in the study are doing is not illegal. They are free to set their own packaging for their own products. But it's just another example of how pharmaceutical companies will stretch the law – and sometimes break it – to make an extra dollar, no matter the cost to others.

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This is a calendar of all of the Weekend or longer Blues/Fusion dancing events in Europe that we know about. Please contact us if you want your event included in the list!
For Pure/Trad Blues event, please check out Annette's excellent Blues in Europe Calendar.
We are quite flexible with our definition. If your event includes "Fusion" (i.e. mixing things but like blues dancing to non-blues music) then you can be on our list!


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Nebraska football commit rumors pointing to new school
Top100 CB Brendan Radley Hiles head to Oklahoma [Image via 247sports/YouTube]
The Husker recruiting class could be getting a bit worse if rumors of a decommit is accurate
by Tobias Richmond (article) and Gilang Ramadhan (video)
October 29, 2017 at 8:07 PM October 29, 2017 at 8:07 PM
Nebraska football commit rumors pointing to new school - Video
The Nebraska football team has had a rather up and down 2017 season. The rollercoaster of emotions Cornhusker fans are likely feeling on Sunday might have just taken a rather big downturn. One of the biggest recruits in the Huskers 2017 recruiting class just visited one of Nebraska's biggest rivals and now there are more than a few recruiting experts who believe that school might have the upper hand.
Brendan Radley-Hiles, better known as "Bookie" among Nebraska football fans, took a trip to Norman over the weekend.
A few reports suggested the defensive back recruit thoroughly enjoyed what the Sooners had to show him. 247Sports has even gone so far as to issue quite a few of what they call their "Crystal Balls," now claiming Bookie is headed to Oklahoma.
Nebraska football losing its grip?
The big question that Husker fans need to ask themselves is how many of these rumors are really true. Bookie had been talking about taking visits almost right after the season started. This was despite the fact that he's been a long time Husker commit.
So far, he's remained a member of the Cornhusker recruiting class, despite the massive amount of attention he's been getting from other schools. The problem is that the chances he might leave, even if he currently doesn't have an interest in doing so, could increase over the course of the season.
Uncertainty surrounding the Cornhuskers
When the Huskers were down by 12 to Purdue, there were few Husker fans who believed mike riley was going to get another season.
Even with the come from behind win, there are few people who believe he has much of a shot at being the coach in Lincoln in 2018.
While fans are excited about the prospects of a new head coach, one thing they don't take into account is the very real effects a change at the top is going to have on recruits. Several of the players the Huskers are looking to reel in have talked about the relationships they have forged with the coaching staff.
There is certainly the old adage that a player commits to a school and not a coaching staff. That adage tends to ignore the fact that players are real human beings. While they are committing to the school, they are likely committing because of the coaches.
If the Nebraska football team does fire Mike Riley and company, they should expect at least some defections from those that have committed. It appears that if things go down the wrong way, Bookie could be one of those defections.
'Call of Duty: Modern Warfare' Season 1 has been extended and a new weapon is coming
Stefania Farah
Gilang Ramadhan
Blasting News recommends Popular 'Fortnite Battle Royale' streamers react to Ninja's official skin 'Fortnite' players can win 25,000 V-Bucks and a VIP package from the new contest Pro player discovers a game-breaking exploit in 'Call of Duty: Modern Warfare' 'Fortnite': New Liferun Mode has officially been announced and it has more vehicles Tfue, DrDisrespect, TimTheTatman react to Ninja's official 'Fortnite' skin Video Samsung on potential Galaxy skin in 'Fortnite' Video


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Q: Differential equation $x'=t^2 \tan x$ $x'=t^2 \tan x$
I tried to do it like a equation with separated variables but the integral was too difficult so probably I have to do it in the other way but I have no idea how right now.

A: $$\cot x\,dx=t^2\,dt\implies \int \cot x\,dx=\int t^2\,dt\implies \ln|\sin x|={t^3\over 3}+C$$


Syracuse University Press, 2009. ISBN 978-0-815-60919-3.
Voted best novel of the year in 2006 by the International Alexandria Library, The Pistachio Seller by Reem Bassiouney is now translated from Arabic so that English readers can enjoy a delightful read.
This story begins with adolescent love as Wafaa, a young Egyptian girl, says with a sense of fun and humor: "It was Saturday. I remember. And while he was standing on a step ladder in the hall, changing a light bulb in the faint light coming through the window, I decided to love him."
Raised in a strict Islamic culture, young Wafaa struggles to come to grips with her own beliefs and the confusing conflicts of a young coming of age body. She meets her cousin Ashraf when he visits from England and develops a healthy respect and growing admiration for her world-traveled and educated older cousin.
Bassiouney lends much factual detail and precise description of the Islam and Egyptian cultures to her story and treats touchy subjects with realism and light humor. The characters are so well defined as to believe the story to be a true narrative of the characters. At times, I wanted to laugh out loud at the amusing thoughts and conversations that two adverse upbringings created in Wafaa and Ashraf. Other times I wanted to slap the characters for their actions and attitudes.
Read The Pistachio Seller through to the end to see how the characters grow and inter-relate with each other and society. Does Wafaa get her man? Read it to see if she does and learn more about the Islamic culture and have fun doing it.
Reem Bassiouney is an acclaimed contemporary Arabic writer. She has published five novels in the Middle East and is an assistant professor of Arabic at Georgetown University in Washington, D.C. This is her first introduction to an English audience.


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Home Videos Renzo Piano Interview: On the Shoulders of Giants | Presented by Louisiana Channel
Renzo Piano Interview: On the Shoulders of Giants | Presented by Louisiana Channel
by Lewis Lewis April 13, 2018
The Louisiana Channel brings you an in-depth biographical interview with the Pritzker prizewinning Italian architect Renzo Piano – known for celebrated buildings such as The Shard and Centre Georges Pompidou – who explains why it's okay "to steal" as long as you give something back.
The Shard in London | Designed by Renzo Piano
"What keeps people alive is not what you've done, what you've been, but what you will be and what you will do." Piano feels that one must avoid falling into the trap of nostalgia by thinking too much about one's roots and past. Born in Genoa, he feels that the sea and its connotations are part of what shaped him: "The sea is like a mysterious place to go one day, so you grow up with this idea to run away one day, and to discover the rest of the world." Moreover, compares the sea to a soup, "a consommé of different cultures."
The Whitney Museum of American Art at Gansevoort. © Nic Lehoux
"It's very funny, because as an architect, at a certain age, when you travel you feel at home everywhere." Piano, who considers himself to be a European rather than an Italian, feels that that travelling is extremely important, because it allows you to get away from what you're doing, permitting you to see it more clearly when you return. As an architect, you can't simply be "a tourist", but you need to understand and listen – not only to people, but also to places, as places too have a story to tell. In continuation of this, he emphasizes that "young people should travel to understand how lucky they are to be born in a place where you live on the shoulders of giants. You live on the freedom that was build up in centuries." If you don't go away, if you don't travel, you don't understand how lucky you are. Moreover, it is important that you appreciate that diversity is a value, not a problem, and what makes us grow, learn – and steal: "Stealing, I know, is not nice, but if the condition is that you give back, it's not that bad." When young people come to work at Piano's offices, what they're told is to "take, take away – don't wait for us to give you, take. But if possible, give back one day."
Astrup Fearnley Museeet © Nic Lehoux
"You are not just a builder, you are also a civic person, so you make a shelter for human beings and human communities. And this becomes even more interesting, because then you make buildings that are for people to stay together and to share values, which is the beginning of maybe making a better world."
Centre Georges Pompidou.
© conservapedia.com
"Architects don't change history, but they witness the change of history." Architects give a shape to the change, which is why public buildings are so important and apart from being good craftsmen, architects need to master the social aspect: In continuation of this, though the war didn't affect him directly, Piano (b. 1937) grew up with a pacifistic attitude, which has stayed with him ever since: "Making a great building is a civic gesture – a gesture of peace."
Renzo Piano (b. 1937) is a lauded Italian architect. His most known buildings include the Centre Georges Pompidou in Paris, The Shard in London, Astrup Fearnley Museum of Modern Art in Oslo, Potsdamer Platz in Berlin and the Whitney Museum of American Art in New York City. In 1998, Piano won the highly prestigious Pritzker Architecture Prize, the jury comparing him to Michelangelo and Leonardo da Vinci, praising him for "his intellectual curiosity and problem-solving techniques as broad and far-ranging as those earlier masters of his native land," and crediting him with "redefining modern and postmodern architecture." In 2006, Piano was selected by TIME as one of the 100 most influential people in the world.
For more see: http://www.rpbw.com/
Text and video courtesy of Louisiana channel
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(September 2016) – For most of us, the closest we have gotten to a torch relay is watching one on TV during the Olympics opening and closing ceremonies. But for 2,200 Hoosiers – 18 of them from Jefferson County, Ind. – the honor of carrying the Indiana Bicentennial Torch will become a reality in September.
Hand-picked by a committee of local residents and approved by state officials, these 18 local residents will share the honor of carrying the Indiana Bicentennial Torch through the Jefferson County on Friday, Sept. 16 – from the county border with Jennings County on Hwy. 7 to the north, all the way to downtown Madison and winding their way through town, ending at the Jefferson County Courthouse, where a ceremony is planned that evening. The Indiana Bicentennial Mobile Experience interactive trailer also will be waiting for them at the courthouse, offering the public a chance to view the displays on the history of the state from 4-8 p.m.
The train car will depart from the Dupont Post Office and travel south to the Madison hilltop, stopping at 6:45 p.m. at the Mayflower building near the No. 5 Fire House on Allen Street and Green Road. A program is planned to take place there at that time to include a welcome by Madison Mayor Damon Welch and a program featuring musician and railroad enthusiast Steve Jeffries and re-enactors portraying John Brough and John Robinson, two figures who played prominent roles in the early days of the railroad in Indiana.
• The torch enters Jefferson County from Jennings County on Hwy. 7. Torch runner Tryston Wheatley runs it to the Dupont Post Office, where it is taken aboard a restored passenger train car pulled by the Madison Railroad.
• 10 torch bearers take turns holding the torch during the train ride from Dupont to Madison, ending at Green Road and Lanier Drive. They include (in order) Spence Schnaitter, Al Huntington, Jim Lee, Susan Stahl, Matt Forrester, Dave Adams, Ray Black, John Staicer, Linda Ferguson and Kim Mahoney.
• Sue Livers takes the torch from the train depot and runs it down Green Road, turning right onto Michigan Road to the top of the Michigan Road Hill.
• Livers hands off to Calista Spears, who runs the torch down the hill and onto West Street to the corner of Third Street at the Volunteer Fire Co. No. 2 station. It is considered to be the oldest still-operating firehouse in the country.
• John Schoenstein takes the torch and boards the 191916 Ahrens-Fox Service Ladder fire truck and rides with it to Main Street, stopping at the public parking lot at 222 W. Main St.
• James Lee takes the torch and runs west on Main Street to Plum Street, passing by the Jefferson County Public Library Main Branch at 420 W. Main St. It is considered to be the first public library in the state. Lee continues south on Plum to First Street, turns east to the Lanier-Madison Visitors Center.
• Trinity Stoner takes the torch south to Vaughn Drive and heads east, passing by the Lanier Mansion, to the Madison Boat Ramp.
• Bert Fitzgerald is tentatively scheduled to take the torch aboard a vintage hydroplane for one loop in the Ohio River.
• Returning to the boat ramp, the torch will be carried by horseback by Bill Gray to the Jefferson County Courthouse, paying tribute to the Canaan-Madison Pony Express Run. He will pass by the Madison Post Office – one of the state's oldest – at the foot of Jefferson Street. It will also pass the location of the first bank in the state, the Farmers' and Mechanics' Bank of Indiana at 310 Jefferson St. and established in 1814.
• Gray will arrive at the Courthouse, where an 8 p.m. ceremony will take place within sight of the state's first firehouse, the Madison Fair Play Fire Co. No. 1 at 405 E. Main St. The torch will depart Jefferson County on Saturday morning and head east on Hwy. 56 into Switzerland County.
Those riding the train and taking turns holding the torch while standing on the back outside rail will be Spence Schnaitter, Al Huntington, Jim Lee, Susan Stahl, Matt Forrester, Dave Adams, Ray Black Jr., John Staicer, Linda Ferguson and Kim Mahoney.
The remaining seven torch bearers will actually run or walk the torch from the train stop on the hilltop to the downtown and wind their way up Main Street and down to the Ohio River and back up Jefferson Street, ending at the Courthouse. These runners include (in order) Sue Livers, Calista Spears, John Schoenstein, James Lee, Trinity Stoner, Bert Fitzgerald and Bill Gray.
Along the way, Schoenstein will do his part by holding the torch while riding aboard a 1916 Ahrens-Fox Service Ladder fire truck, owned by local resident Frank Taff. He will board the fire truck at the No. 2 Fire House on Third and West streets and then ride west on Main Street to the city parking lot across from the Comfort Station. From there, runners will take over on foot again heading south on Plum Street, east on First Street to the Lanier Mansion at Vine Street. While passing the mansion on the way to the riverfront, cannons will be fired by the 7th Indiana Light Artillery and Nelson Artillery Co.
When the torch arrives at the Madison Boat Ramp, tentative plans are to have Fitzgerald hold the torch while taking a loop in the Ohio River aboard a vintage hydroplane. Finally, the last torch bearer, Gray, is scheduled to ride up Jefferson Street carrying the torch aboard a horse to pay tribute to the Canaan-Madison Pony Express Run (See Torch Route graphic for details).
The torch route was carefully planned by a small committee of local residents and led by Linda Lytle, executive director of VisitMadison Inc. and the county's designated Indiana Bicentennial Commission coordinator, and Andrew Forrester, Community Relations Director for the City of Madison.
"We are hoping lots of people come out to watch the torch runners and cheer them on as they go through town," Lytle said.
She explained that the committee devised the torch relay route to go past several historic sites in the downtown. These include three volunteer firehouses including the Fair Play No. 1 station, considered to be the oldest one still in use in the state. Other notable sites are the Jefferson County Public Library, the oldest library in the state; the Lanier Mansion Sate Historic Site, the Madison Post Office, the state's oldest; and the location of the first bank in the state, the Farmers' and Mechanics' Bank of Indiana at 310 Jefferson St. and established in 1814.
"I think it is important that we support the torch runners as they go through town, and we made a special effort in creating the route to highlight the significance of these historic locations," Lytle said.
Livers, 67, will be the first torch runner in Madison after the torch departs the train. She will carry it all the way to the top of Michigan Road hill, where she will hand off to Spears. Livers recently attended a torch relay training session in Brownstown, Ind., where a video was played to teach torch bearers how to carry the flame safely. She was allowed to hold the actual torch and see the yellow shirts and hats each runner will be wearing.
Livers learned several things about the torch during her training. She said the torch weighs 3½ pounds. The torch relay procession will be preceded by two Indiana State Police cars and trailed by two more police cars. Driving immediately in front and behind the runner will be representatives from Purdue University, who not only created the torch but are there to ensure that it stays lit and also for any emergencies related to the torch.
Engineering students from Purdue University created the Olympic-style torch that will be carried 2,000 miles through all 92 Indiana counties in September.
Lillian Sue Livers holds the Indiana Bicentennial torch during a training meeting in August in Brownstown, Ind. She was given safety tips on how to carry the 3 1/2 pound torch.
By downloading the "Indiana Bicentennial Torch 2016" app on a cell phone, users will be able to also follow the torch relay.
Lytle said more than 50 people were nominated as torch bearers for the county. A maximum of 20 runners and two substitutes were allowed to be selected. The committee offered 23 people the chance to participate, but "a couple of people who we selected chose not to participate, so we ended up with 18," she said.
The selection committee for the torch bearers was made up of Bob Canida, Laura Hodges, Joe Craig, John Nyberg and Treva Shelton. "It was a good process; it's been a fun experience," Forrester said, who recused himself from the selection committee since his father, Matthew, was nominated and later selected.
Roger Fuehring has restored this 1912 Pullman Standard premium train car at the Madison Railroad. Ten torch bearers will ride in the car from Dupont to Madison, each taking turns holding the Indiana Bicentennial torch on the back platform.
One torch runner in that category is Schoenstein, 36, a fulltime employee at Madison Chemical, a part-time Jefferson County Sheriff's officer in charge of the reserve unit, and a volunteer at two Madison fire departments. He was surprised by his selection because his friend who nominated him "did a pretty good job of keeping it a secret for seven months," Schoenstein said.
In addition to the Bicentennial Torch Relay that Friday, the committee has organized a weekend full of activities for the community, including a "Passport" that will allow people to tour the county's historic sites for free. The Historic Madison Inc. sites – Schroeder Saddletree Factory, Dr. Hutchings' Office, Francis Costigan House and the Jeremiah Sullivan House – plus the Lanier Mansion and the Jefferson County History Center will be open to the public for free that Saturday from 10 a.m. to 3 p.m. The Eleutherian College in Lancaster, Ind., will be open for free from 1-5 p.m. Family activities also are planned at John Paul Park from 10 a.m. to noon and again at 4 p.m. when the Daughters of the American Revolution will conduct a bell ringing in conjunction with the local churches.
The Passport to visit these sites for free will be available at the Lanier-Madison Visitors Center, 601 W. First St., or at any of the participating historic sites. Costumed characters will appear at many of these sites, and special period events are being planned for that Saturday. Those visitors who fill their Passports becoming eligible for a prize drawing totaling $300.
"We want to use this opportunity to put the spotlight on Madison and all it has to offer, not only to visitors but to residents as well," Lytle said. The Passport, she added, offers anyone a chance to visit and learn about the county's unique history.
Meantime, many other activities are planned throughout town that weekend. Saturday events include the Madison Farmers' Market at the Broadway Fountain (7 a.m. – 1 p.m.); an Architectural Walking Tour beginning at the Broadway Fountain (10 a.m. – noon); A Heritage Sites Tour (10 a.m. – 5 p.m.); Vintage Hydroplane exhibition boat races (11 a.m. – 5 p.m. Saturday and Sunday at the riverfront); Hispanic Cultural Awareness Day (4-9 p.m. at the Broadway Fountain; and music by the Madison Community Band at 6:30 p.m. at Madison Bicentennial Park, followed by the showing of the movie "Hoosiers" at dusk (bring chairs or blankets).
Sunday's activities include two plays to be performed for free by the Madison Community Players beginning at 3:30 p.m. at the Jefferson County History Center, 615 W. First St. Both plays will highlight life and times of famed voting rights activist Susan B. Anthony. The first play, "The Remarkable Susan," is a one-act drama written by playwright Tim Kelly. The second production was written by Madison resident Jan Vetrhus and is titled "Susan B. Anthony Comes to Madison" and is based on her visit to Madison in 1879.
• For more information on the Indiana Bicentennial, visit www.Indiana2016.org. For questions about bicentennial events in Jefferson County, call VisitMadison Inc. at (812) 265-2956.


Offense, i am more of a playmaker and i play to make the field bigger and make players open.
Well idk how to answer this but i think it is good because i have had a character before this.
Like i said i had a lvl 100 before and i knew the pmc since then.
I know alot of the members and thats chemistry.
FC Nemean Lions staff have decided to reject your application.
Good luck in your search for a PMC.


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Home 'The Fiddling Horse' Film Premiere
'The Fiddling Horse' Film Premiere
Zachary High School Visual and Performing Arts Center 4100 School St, Baton Rouge, Louisiana 70791
the fiddling horse film
Leslie Heart fears that she may be losing status within her high society circle of friends, so when she finds out that she's inherited a racehorse, she teams up with an ex-celebrity jockey to execute a con to cash in on the monetary and social gains of the racecourse. Directed by CJ Wallis and shot on location in Louisiana, "The Fiddling Horse" will enjoy is southern premiere this month at the Zachary High School Visual and Performing Arts Center, starring stand-up comedian Andy Kindler ("Everybody Loves Raymond," "Bob's Burgers," "I'm Dying Up Here"), J. Elvis Weinstein ("Mystery Science Theater 3000," "Freaks and Geeks"), Paula Lindberg ("Eureka"), Alley Mills ("The Wonder Years," "The Bold and the Beautiful"), David Haydn-Jones ("Supernatural"), Billy Mitchell ("King of Kong"), Johnny Territo, and Heather Matarazzo ("The Princess Diaries," "Welcome to the Dollhouse," "The L Word"). Don't miss out on this dark comedy straight from the Pelican State. $10. Doors open at 6 pm. eventbrite.com. Check out the trailer here.
Location Zachary High School Visual and Performing Arts Center 4100 School St, Baton Rouge, Louisiana 70791
Regions Greater Baton Rouge
Event Type Films
Date & Time Dec 12, 2019


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Q: remove unused files from storage I saved some images in my storage's specific folder.I have fro example 1.png,2.png and etc. I know how i can get all files's name.This is source
  private void getAllElemetsFromStorage() {
    String root_sd = Environment.getExternalStorageDirectory().toString();
    File file = new File(root_sd + "/myfolder");
    for (File f : file.listFiles()) {
        if (f.isFile()) {
            String name = f.getName();
            Log.e("file names", name + "");
        }}
}

This code working correct but i have one problem.I have some json and in my json i have file's name.How i can get all files name witch is not in my json and is my directory and how i can delete all this files? My goal is to save only files,witch are in my jsons  and i want to delete all unused files from my directory
How i can solve my problem?
thanks

A: Inside your if statement, after you get the file name, loop through the json and check whether its in there or not. If not, delete it.
Your for loop that exists already will do this for every file in the directory, removing it if the name doesnt exist in the json.
Below is an example. Depending on your Json, you need to build a list or loop through another way.
private void getAllElemetsFromStorage() {
  String root_sd = Environment.getExternalStorageDirectory().toString();
  File file = new File(root_sd + "/myfolder");
  ArrayList<String> jsonFileNames = // Get list of file names from json

  for (File f : file.listFiles()) {
    if (f.isFile()) {
        String name = f.getName();

        // If not found in json. Delete file
        if(!jsonFileNames.contains(name))
           f.delete();
    }
  }
}

Note: this code is untested so may be typos. But it should give you the idea.


The ultimate Oregon coast tent trailer adventure is something you have to do this year, all 500 miles of it. It's a three to five day overlanding adventure featuring the very best wild and scenic Oregon. Rent your adventure tent trailer today!
The North Coast is wild. It has the longest stretches of sandy beaches (some you can camp on!) and is the most visited part of the Oregon Coast during summer, but fall and winter this place is all yours. It's most well known for Cannon Beach and scenic Haystack Rock plus adventures from hikes to zip lines.
Lewis and Clark National and State Historical Parks / Fort Clatsop National Park unit.
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Glenn Robbins
Glenn Robbins , a graduate of Drama and Media at Melbourne State College, first moved into performing in 1981. As a stand-up comedian, he enjoyed performing at popular comedy venues in Melbourne and Sydney. Audiences warmed to his naturally dry...
Glenn Robbins Travels from VIC
Glenn Robbins's Biography
Glenn Robbins , a graduate of Drama and Media at Melbourne State College, first moved into performing in 1981. As a stand-up comedian, he enjoyed performing at popular comedy venues in Melbourne and Sydney. Audiences warmed to his naturally dry sense of humour and style.
The move into television was a natural progression for Glenn Robbins. He became well-known as a performer/writer for a number of television's top rating comedy sketch shows including: 'THE COMEDY COMPANY' (Network Ten), 'FAST FORWARD', 'FULL FRONTAL' and 'JIMEOIN' (all 7 Network). While he performed a good many characters throughout these shows, Glenn's most prominent and notable would be that of Uncle Arthur .
A regular guest on channel 7's top rating 'TONIGHT LIVE', Glenn Robbins often appeared, from various locations around the country, presenting his live Talk Cams.
In 1996, Glenn enjoyed a successful season of live performances of 'The Cooking Show' at The Edinburgh Festival, once again teaming up with fellow comedians Jimeoin and Bob Franklin.
A regular member of the Working Dog production team, Glenn appeared on (Network Ten) " THE PANEL" from 1998-2004. With Working Dog , Glenn also created the outback adventure parody "ALL AUSSIES ADVENTURES" with Russell Coight , series 1 and 2 (also Network Ten). In the very popular "THANK GOD YOU'RE HERE" series, Glenn has the dual role of Creative Consultant as well as having performed in a couple of episodes.
IN 2001, Glenn played the role of Pete Morrison in the much-acclaimed Australian feature film, "LANTANA". This AFI award winning film, directed by Ray Lawrence, has seen both local and international success.
2002 saw Glenn Robbins, a.k.a. Kel Knight, alongside Jane Turner and Gina Riley, in the AFI award winning comedy series "KATH & KIM" (ABC TV). So enormously successful is Kath & Kim, that a further 2nd and 3rd series were produced for TV during 2003/2004 and, as it gathered international recognition, particularly in Britain and USA, a Kath & Kim tele-movie was produced for broadcast in 2006.
That same year, Glenn Robbins played the leading role of Benny G in Molloy Boys' feature film, "BOYTOWN" – the story of a successful 80s boy band who decide to reform in the hope of recapturing some of their former glory.


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Q: Is there a way to override system name for Java app? There is a Java Web Start application that I'm trying to run under Java on Linux. I'm using icedtea-netx on Ubuntu Linux.  When I try to run the application, it starts up, shows the splash screen, then produces an error saying:

"Currently the application only supports the following system: Windows".

So I'm wondering, is there a way to set your system information in Java to pretend that it's Windows?  I understand that this program might really require some aspect of Windows, but I'd like to try anyways. Thanks.