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

`Very low mass stars' (VLMS), with masses between 0.08 and $0.3\,M_\odot$, are the most dominant subset of the stellar population \citep[e.g.][]{2001MNRAS.322..231K}. These stars are thought to have fully convective interiors and hydrogen fusion in their cores, distinguishing them from higher mass stars and brown dwarfs, respectively \citep[see review by][]{2000ARA&A..38..337C}. Mass and radius are two of the most fundamental measurements for stars. Previous studies have shown that the radii of sub-solar mass stars are under-predicted by theoretical interior models at the $5-10$\% level \citep[e.g.][]{2002ApJ...567.1140T,2006Ap&SS.304...89R,2010A&ARv..18...67T,2012ApJ...757...42F,2013ApJ...776...87S}. The interior structure of the fully convective VLMSs is different to that of higher mass, partially radiative stars, and therefore warrants a more thorough, independent examination.

The vast majority of masses and radii come from dynamical measurements of binary systems. One explanation for the radius anomaly is that these M-dwarf binaries are spun-up by tidal interactions, the speed-up of the internal dynamo then leads to increased magnetic activities, suppressing convection and increasing star-spot activity \citep[e.g.][]{2006Ap&SS.304...89R,2005ApJ...631.1120L,2007ApJ...660..732L,2010ApJ...718..502M}. \citet{2007A&A...472L..17C} showed that the general radius discrepancies for low mass stars can be accounted for by allowing large spot coverages and varied mixing length in the models. However, since the magnetic field is thought to be generated differently in fully convective stars \citep[e.g.][]{2006A&A...446.1027C}, the effect of this spin-up on the VLMSs and the resulting spot coverage is unclear. In addition, the effect of the mixing length parameter incorporated in stellar models for fully convective, near adiabatic, stars is significantly less than that for higher mass stars. Any explanation for the radius anomaly should also not be restricted to binaries, since the radius inflation is also observed for isolated M-dwarfs measured via interferometry \citep[e.g.][]{2006ApJ...644..475B,2012ApJ...757..112B,2013ApJ...776...87S}.

It remains difficult to test stellar models for the VLMS population, given that metallicities and precise (better than 10\%) mass radius measurements are available for only 13 previous objects (see Section~\ref{sec:mass-radi-relat}). In contrast, we know the masses and radii of $\sim 40$ exoplanets to better than 5\% precision, which has led to more thorough examinations of planet interior models \citep[e.g.][]{2011ApJ...729L...7L,2012ApJ...744...59S}. The radii of stand-alone, close-by M-dwarfs can be measured via interferometry \citep[e.g.][]{2003Aamp;A...397L...5S}, but the masses must be inferred from empirical mass-luminosity relationships. Dynamical masses of binaries can be obtained via astrometric orbit measurements \citep[e.g.][]{2013ApJ...773...28S}. Double-lined M-M eclipsing binary systems provide accurate, model-independent mass and radius measurements \citep{1996ApJ...456..356M,2011Sci...331..562C,2011Sci...333.1602D,2011ApJ...742..123I,2013MNRAS.tmp.1072N}, but these systems are relatively rare. In addition, the accuracy of M-M binary derived system parameters may suffer from M-dwarf activity and unaccounted spot variability, and may not be as reliable as previously thought \citep{2012ApJ...757...42F}.

Photometric transit surveys have lead to a rapid expansion in the population of transiting exoplanets. VLMSs have radii comparable to that of gas-giant planets, and are often found as companions in binary systems to solar-type stars. These F-M binaries exhibit similar transit signals as hot-Jupiter systems, and can be easily identified by transiting planet surveys. The population of well characterised VLMSs can be greatly extended by including single lined F-M binaries \citep[e.g.][]{2005A&A...433L..21P,2006A&A...447.1035P,2007ApJ...663..573B,2009ApJ...701..764F,2013Aamp;A...549A..18T}.

There are a number of approaches towards measuring the mass and radius of M-dwarf companions in single lined F-M binary systems. The primary star properties can be obtained by combining spectroscopic analysis with stellar evolution models. The precision of the measured companion mass and radius are limited by the uncertainty in the primary star properties. For orbital companions of substantial mass, the rotation of the primary star is quickly synchronised with the companion orbital period. Fundamental system parameters derived from transit light curves, combined with rotational velocities measured from spectra, can yield relatively model-independent masses and radii for both components of a binary system \citep[e.g.][]{2007ApJ...663..573B,2009ApJ...701..764F}.

In this study, we present the discovery of four single-lined stellar systems with 0.1--0.2\,$M_\odot$ VLMS companions. These low mass eclipsing binaries were identified by the HATSouth survey \citep{2013PASP..125..154B}. The discovery and follow-up observations are detailed in Section~\ref{sec:observations}. Analysis of the individual systems, including spectral classifications of the primary star, global modelling of the light curves and radial velocity data, and descriptions of the methods used to derive the mass and radius of the companions, can be found in Section~\ref{sec:analysis}. Section~\ref{sec:discussion} discusses these new discoveries in the context of existing VLMS systems, and examines the mass-radius anomaly in the VLMS regime.

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

\subsection{HATSouth photometric detection}
\label{sec:hatsouth-detection}

The transiting VLMS systems were identified from photometric observations by the HATSouth global network. HATSouth consists of six telescope units spread over three sites, Siding Spring Observatory (SSO) in Australia, Las Campanas Observatory (LCO) in Chile, and the HESS site in Namibia, providing continuous monitoring of 128 deg$^2$ fields in the Southern sky \citep{2013PASP..125..154B}. Each unit consists of four 0.18\,m f/2.8 Takahasi astrographs and  Apogee Alta-U16M D9 $4\text{k}\times4\text{k}$ front illuminated CCD cameras, with $9\,\mu\text{m}$ pixels, and plate scale of $3.7" \, \text{pixel}^{-1}$. The four telescopes are offset by $4^\circ$, allowing four adjacent $4^\circ \times 4^\circ$ fields to be simultaneously monitored. The observations are made at 4 minute cadence in the $r'$ band. Each field is monitored for $\sim 2$ months by a unit at each HATSouth station. Aperture photometry is performed on the reduced frames, and detrended using External Parameter Decorrelation \citep[EPD,][]{2007ApJ...670..826B} and Trend Filtering Algorithm \citep[TFA,][]{2005MNRAS.356..557K}. Objects exhibiting periodic transit signals are identified using the Box-fitting Least Squares technique \citep[BLS,][]{2002A&A...391..369K}.

The HATSouth discovery light curves for the systems presented in this study are shown in Figure~\ref{fig:HS_lightcurve}, and are summarised in Table~\ref{tab:phot_obs_tab}. Details of our planetary candidate selection, vetting, and confirmation process can be found in the recent HATSouth publications \citep{2013AJ....145....5P,2013A&A...558A..55M,2013AJ....146..113B}.

\begin{table*}
\begin{center}
\caption{
    Summary of photometric observations
    \label{tab:phot_obs_tab}
}
{\footnotesize\begin{tabular}{lllrr}
\hline
    \multicolumn{1}{c}{Facility}          &
    \multicolumn{1}{c}{Date(s)}             &
    \multicolumn{1}{c}{Filter}      &
    \multicolumn{1}{c}{Number of images}         &
    \multicolumn{1}{c}{Cadence (s)}            \\
\hline
\bf{HATS550-016}\\
    HATSouth & 2009/09/28--2010/12/20 & $r'$ & 8726 & 240\\
    FTS / Merope & 2012/11/17 & $i'$ & 160 & 60\\
    MPG/ESO 2.2\,m / GROND & 2012/12/08 & $g',i',z'$ & 187 & 145 \\
    MPG/ESO 2.2\,m / GROND & 2012/12/08 & $r'$ & 185 & 145 \\

\\
\bf{HATS551-019}\\
    HATSouth & 2009/09/09--2010/04/29 & $r'$ & 5274 & 240\\
    PEST & 2012/12/23 & $R_c$ & 168 & 120 \\
\\
\bf{HATS551-021}\\
    HATSouth & 2009/09/09--2010/04/29 & $r'$ & 5274 & 240\\
\\
\bf{HATS553-001}\\
    HATSouth & 2009/09/17--2010/09/10 & $r'$ & 10703 & 240\\
   PEST & 2012/12/22 & $R_c$ & 92 & 120 \\
\hline
\end{tabular}}
\end{center}
\end{table*}

\begin{figure*}
 \centering
 \begin{tabular}{cc}
 \includegraphics[width=9cm]{plots/550-016/HS_lightcurve.eps} &
 \includegraphics[width=9cm]{plots/551-019/HS_lightcurve.eps} \\
 \includegraphics[width=9cm]{plots/551-021/HS_lightcurve.eps} &
 \includegraphics[width=9cm]{plots/553-001/HS_lightcurve.eps} \\
 \end{tabular}
 \caption{HATSouth discovery light curves of the four VLMS systems, including close-ups of the transit event. The best fit models from Section~\ref{sec:lightcurve-analysis} are plotted in red.}
  \label{fig:HS_lightcurve}
\end{figure*}

\subsection{Identification of stellar mass binaries by ANU 2.3\,m/WiFeS}
\label{sec:recon_spec}

Spectroscopic follow-up of HATSouth candidates start with reconnaissance spectroscopic observations, at high signal-to-noise (S/N) and low--medium resolution, to determine preliminary primary star properties and to search for high amplitude radial velocity variations $(>2\,\text{kms}^{-1})$. These observations allow efficient identification of non-planetary systems, such as F-M binaries, by providing an initial mass estimate for the primary star and any secondary companion found. The reconnaissance observations are summarised in Table~\ref{tab:spec_obs_tab}.

\begin{table*}
\begin{center}
\caption{
    Summary of spectroscopic observations \label{tab:spec_obs_tab}
}
{\footnotesize\begin{tabular}{llrrr}
\hline
    \multicolumn{1}{c}{Facility}          &
    \multicolumn{1}{c}{Date} &
    \multicolumn{1}{c}{Resolution} &
    \multicolumn{1}{c}{Wavelength}          &
    \multicolumn{1}{c}{Number of}\\
    \multicolumn{1}{c}{}          &
    \multicolumn{1}{c}{Range} &
    \multicolumn{1}{c}{} &
    \multicolumn{1}{c}{Coverage (\AA)}          &
    \multicolumn{1}{c}{Observations}\\
\hline
\bf{HATS550-016}\\
    ANU 2.3\,m / WiFeS & 2012/05/11--2012/08/07 & 3000 & 3500--6000 & 2 \\
    ANU 2.3\,m / WiFeS & 2012/08/04--2012/10/31  & 7000 & 5200--7000 & 16\\
    Euler 1.2\,m / Coralie & 2012/08/25--2012/11/11 & 60000 & 3850--6900 & 7\\
    ANU 2.3\,m / Echelle & 2012/12/04--2012/12/06 & 24000 & 4200--6725 & 7\\
\\
\bf{HATS551-019}\\
    Euler 1.2\,m / Coralie & 2010/10/28--2011/02/18 & 60000 & 3850--6900 & 3\\
    ANU 2.3\,m / WiFeS & 2010/11/26--2011/04/19  & 7000 & 5200--7000 & 4 \\
    ANU 2.3\,m / Echelle & 2013/03/23--2013/04/01 & 24000 & 4200--6725 & 7\\
\\
\bf{HATS551-021}\\
    Euler 1.2\,m / Coralie & 2010/10/28-2011/02/18 & 60000 & 3850--6900 & 3\\
    ANU 2.3\,m / WiFeS & 2010/11/26--2011/09/17  & 7000 & 5200--7000 & 3 \\
    MPG/ESO 2.2\,m / FEROS & 2011/09/09-2011/09/10 & 48000 & 3500--9200 & 2\\
    ANU 2.3\,m / WiFeS & 2011/09/17 & 3000 & 3500--6000 & 1 \\
    ANU 2.3 m / Echelle & 2013/03/23--2013/04/01 & 24000 & 4200--6725 & 7\\
\\
\bf{HATS553-001}\\
    ANU 2.3\,m / WiFeS & 2012/05/08 & 3000 & 3500--6000 & 1 \\
    ANU 2.3\,m / WiFeS & 2012/05/09--2012/05/09  & 7000 & 5200--7000 & 2\\
    ANU 2.3\,m / Echelle & 2013/03/23--2013/04/01 & 24000 & 4200--6725 & 7\\
\hline
\end{tabular}}
\end{center}
\end{table*}

Initial spectroscopic observations of the targets were obtained using the Wide Field Spectrograph (WiFeS) on the ANU 2.3\,m telescope \citep{2007Ap&SS.310..255D}, located at Siding Spring Observatory (SSO), Australia.

First, a low resolution ($R \equiv \lambda / \Delta \lambda = 3000$) spectrum covering the wavelength region 3500--6000\,\AA\, was used to obtain an initial stellar classification of the target star. The flux calibrated spectrum was fitted to a grid of synthetic spectra from \citet{2008A&A...486..951G}. Details of the low resolution spectral reduction and analysis, including fitting of the stellar properties, are given in \citet{2013AJ....146..113B}. These stellar parameters are later refined using high resolution spectra (see Section~\ref{sec:host-star-properties}).

Subsequent medium resolution, multi-epoch radial velocity observations were performed with WiFeS at $R=7000$, observed at phase quadratures of the photometric ephemeris, where the potential velocity variation is greatest. In the case of stellar binaries, the radial velocity variations are often apparent with two well-time exposures. Combined with the WiFeS stellar parameters, the WiFeS radial velocity orbit provides an initial mass estimate of the companions and affect their prioritisation for further follow-up studies. The WiFeS velocities were not included in the final system analysis, since fewer, lower resolution observations do not contribute greatly to improving the precision of the measured radial velocity orbit.

\subsection{High resolution spectroscopic follow-up}
\label{sec:high-resol-flup}

Radial velocity measurements derived from high resolution spectroscopic observations were obtained for the VLMS systems using the Echelle spectrograph on the ANU 2.3\,m telescope at SSO; the fibre-fed echelle spectrograph CORALIE on the Swiss Leonard Euler 1.2-m telescope \citep{2000A&A...354...99Q} at La Silla Observatory (LSO), Chile, and the fibre-fed echelle spectrograph FEROS on the MPG/ESO 2.2\,m telescope \citep{1998SPIE.3355..844K} at LSO. The observations are summarised in Table~\ref{tab:spec_obs_tab}. Descriptions of the data reduction and analysis for CORALIE and FEROS can be found in \citet[][Jord\'{a}n et al. in prep]{2013AJ....145....5P}. This is the first time we have used the ANU 2.3\,m Echelle to monitor HATSouth targets, a description of these observations are presented below.

\subsubsection{ANU 2.3\,m / Echelle}
\label{sec:echelle}

High resolution spectra of the systems were obtained using the Echelle spectrograph on the ANU 2.3\,m telescope. The echelle was configured to a 1\farcs8 wide slit, delivering a resolution of $ R = 24000$, velocity dispersion of $4.0 \, \text{km} \, \text{s}^{-1} \, \text{pixel}^{-1}$, in the spectral range 4200--6725\,\AA, over 20 echelle orders. The detector is a $2\text{K}\times 2\text{K}$ CCD with gain of $2\,\text{e}^-\,\text{ADU}^{-1}$ and read noise of $2.3 \,\text{ADU}\,\text{pixel}^{-1}$, and binned $2\times$ in the spatial direction. A number of instrument limitations prevent us from achieving better than $500\,\text{ms}^{-1}$ velocity precision. For example, the instrument is mounted on the Nasmyth focus, not in a temperature stabilised environment; the low efficiency of the spectrograph limits the study to only bright stars $(<13.5\,V_\text{mag})$. The data was reduced with the IRAF\footnote{IRAF is distributed by the National Optical Astronomy Observatories, which are operated by the Association of Universities for Research in Astronomy, Inc., under cooperative agreement with the National Science Foundation.} package CCDPROC, and extracted using ECHELLE\@. A rapidly rotating B star spectrum is divided through each observation to remove the blaze function. A low order spline interpolation is then used to continuum normalise each spectrum. The wavelength solution was provided by Th-Ar arc lamp exposures that bracketed each science exposure.

Radial velocity measurements were obtained by cross correlating the object spectra against a series of radial velocity standard star spectra taken on the same night. The radial velocities derived from selected echelle orders not severely contaminated by telluric absorption features were sigma clipped and weight averaged according to their respective CCF heights and S/Ns. Typically 15 echelle orders were used in the cross correlations. A velocity and the associated uncertainty was determined for each order, from which the weighted average and standard deviation were calculated and adopted as the measured velocity. For stable HATSouth candidates with $V_\text{mag}\approx 13$, the long-term root-mean-squared (RMS) velocity scatter of the instrument is $\sim 1.0\,\text{km}\,\text{s}^{-1}$. Stellar parameters were also derived from the Echelle spectra, the process is described in detail in Section~\ref{sec:host-star-properties}.

\subsection{Photometric follow-up}
\label{sec:phot-flup}

Follow-up photometric confirmations for the transit events of HATS550-016B, HATS551-019B, and HATS553-001B were made using the Merope camera on the 2\,m Faulkes Telescope South (FTS) located at SSO, the Gamma-Ray Burst Optical/Near-Infrared Detector (GROND) on the MPG/ESO 2.2\,m telescope at LSO, and the 0.30\,m Perth Exoplanet Survey Telescope (PEST) located in Perth, Australia. The observations are listed in Table~\ref{tab:phot_obs_tab}, with the light curves plotted in Figures~\ref{fig:fit_550-016}, \ref{fig:fit_551-019}, \ref{fig:fit_553-001}.

\subsubsection{FTS 2\,m / Merope}
\label{sec:fts-phot}

A near-full transit for HATS550-016B was observed on 2012 November 17 using the Merope imaging camera on the 2\,m Faulkes Telescope South, part of the Las Cumbres Global Telescope (LCOGT) Network. Merope is a $2\text{K} \times 2\text{K}$ camera with $0.139\text{"}\,\text{pixel}^{-1}$ pixels, binned at $2\times2$, and a FoV of $4.7\text{'}\times4.7\text{'}$. The observation was performed in the SDSS $i'$ band, with 60s exposure time, and the telescope slightly defocused to reduce pixel-pixel and imperfect flat field systematic effects and to prevent saturation. The data was reduced by the automated LCOGT pipeline.

Aperture photometry was performed on the reduced images with Source Extractor \citep{1996A&AS..117..393B}. Stellar flux was extracted over multiple diameter apertures, reference stars are selected based on their brightness, colour, and lack of blended neighbours.

\subsubsection{MPG/ESO 2.2\,m / GROND}
\label{sec:grond}

A full transit for HATS550-016B was also observed on 2012 December 08 using GROND on the 2.2\,m MPG/ESO telescope at LSO. GROND provides simultaneous multi-band photometry in four optical bands similar to Sloan $g'$, $r'$, $i'$, and $z'$. It has a field of view of $5.4\text{'} \times 5.4\text{'}$ with $0.158\text{"}\,\text{pixel}^{-1}$ pixels. Exposure times for the HATS550-016 observations were 100s. Details of the GROND observing strategy and data reduction procedure can be found in \citet{2013AJ....145....5P,2013A&A...558A..55M}.

\subsubsection{PEST}
\label{sec:tg30cm}

A full transit of HATS553-001 and a partial transit of HATS551-019 were observed using PEST on 2012 December 22 and 2012 December 23 respectively. PEST is a fully automated 0.30\,m Meade LX200 Schmidt Cassegrain telescope located at latitude $-31^\circ\, 59\text{'} \, 34\text{''}$, longitude $115^\circ \, 47\text{'} \, 53\text{''}$E. The telescope is coupled with a focal reducer to yield a focal ratio of f/5. The detector is a SBIG ST-8XME CCD camera with gain of $2.27\,e^{-}\,\text{ADU}^{-1}$ and read noise of $19.9\,e^{-}$, with image scale of $1.2\text{''}\,\text{pixel}^{-1}$, and a FoV of $31\text{'} \times 21 \text{'}$. Images were taken in the $Rc$ band, with the telescope in focus, exposure times are provided in Table~\ref{tab:phot_obs_tab}. Typical conditions yield stellar point-spread-functions with FWHM of $\sim 3$ pixels. Flat field frames are taken in twilight whenever possible. Dark frames of equal exposure length to the object frames are drawn from a library of master dark frames, renewed every month.

Image reduction and aperture photometry were performed using the C-Munipack program. Relative photometry is performed, with the reference light curve made from the weighted average of high S/N field star light curves.

\section{Analysis}
\label{sec:analysis}

\subsection{Fundamental stellar atmospheric parameters}
\label{sec:host-star-properties}

The fundamental primary star properties, including effective temperature (\teff), surface gravity ($\log g$\xspace), metallicity ([Fe/H]\xspace), and projected rotational velocity ($v \sin i_\text{rot}$\xspace), were derived by fitting synthetic model spectra to the averaged ANU 2.3\,m / Echelle observations. We generated a synthetic spectral library with the ATLAS9 model atmospheres \citep{2004astro.ph..5087C}, using the spectral synthesis program SPECTRUM\footnote{\texttt{http://www1.appstate.edu/dept/physics/spectrum/spectrum.html}} \citep{1994AJ....107..742G}. The spectra have resolutions of $R=24000$, matching that of the Echelle instrument, and were generated at the ATLAS9 \teff, $\log g$\xspace, and [Fe/H]\xspace grid points, using the default isotopic line lists provided with SPECTRUM, then broadened to multiple rotational velocities spaced 5\,\mbox{km\,s$^{-1}$}\xspace apart. Model microturbulences are fixed at 2\,\mbox{km\,s$^{-1}$}\xspace, given that the range of possible microturbulence values for the \teff and $\log g$\xspace tested varies only by $\sim 0.5\,\text{km}\,{s}^{-1}$ \citep{2013A&A...553A...6H}. The individual echelle orders of the observed spectrum were matched to a restricted grid, centred about the rough stellar parameter estimates from the WiFeS spectrum. Using exposures of standard stars, we found echelle orders that gave the most reliable stellar parameters for a target of a given spectral type. The fitting results from these selected orders were weight averaged according to their RMS scatter from the fit.     The $\log g$\xspace was subsequently constrained from theoretical isochrones (see Section~\ref{sec:lightcurve-analysis}) via global light curve and radial velocity modelling. We then performed the grid search again, at a finer $v \sin i_\text{rot}$\xspace grid of 1\,\mbox{km\,s$^{-1}$}\xspace spacings, with $\log g$\xspace fixed, to obtain the final stellar parameters. The primary star parameters are presented in Table~\ref{tab:host-star}.

\begin{table*}
\begin{center}
\caption{
    Primary star properties \label{tab:host-star}
}
{\footnotesize\begin{tabular}{lrrrr}
\hline
    \multicolumn{1}{c}{Property}          &
    \multicolumn{1}{c}{HATS550-016} &
    \multicolumn{1}{c}{HATS551-019} &
    \multicolumn{1}{c}{HATS551-021} &
    \multicolumn{1}{c}{HATS553-001} \\
\hline
GSC$^{a}$ & 6465-00602 & 6493-00290 & 6493-00315 & 5946-00892 \\
RA$^{b}$ (J2000 HH:MM:SS.SS) & 04:48:23.32 & 05:40:46.16 & 05:42:49.12 &06:16:00.66 \\
DEC$^{b}$ (J2000 DD:MM:SS.SS) & -24:50:16.88 & -24:55:35.16 & -25:59:47.49 & -21:15:23.82\\
\\
\multicolumn{4}{l}{\bf{Photometric Properties}}\\
$V$$^{c}$ & $13.605\pm0.041$ & $12.058\pm0.006$ & $13.114\pm0.008$ & $13.189\pm0.021$\\
$B$$^{c}$ & $14.052\pm0.020$ & 12.497 & $13.580\pm0.012$ & $13.694\pm0.014$\\
$g'$$^{c}$ & $13.782\pm0.032$ & 12.198 & 13.308 & 13.408\\
$r'$$^{c}$ & $13.499\pm0.031$ & 11.953 & $13.044$ & 13.102\\
$i'$$^{c}$ & 13.438 & $11.922\pm0.038$ & $12.985\pm0.077$ & 13.988\\
$J$$^{b}$ & $12.640\pm0.021$ & $11.146\pm0.021$ & $12.150\pm0.021$ & $12.245\pm0.021$\\
$H$$^{b}$ & $12.379\pm0.025$ & $10.943\pm0.024$ & $11.956\pm0.020$ & $12.023\pm0.025$ \\
$K$$^{b}$ & $12.308\pm0.021$ & $10.914\pm0.021$ & $11.873\pm0.023$ & $11.970\pm0.024$ \\
\\
\multicolumn{4}{l}{\bf{Derived Spectroscopic Properties}}\\
\teff\,(K) & $6420\pm90$ & $6380\pm170$ & $6670 \pm 220$ & $6230\pm250$ \\
[Fe/H]\xspace & $-0.60\pm0.06$ & $-0.4 \pm 0.1$ & $-0.4 \pm 0.1$ & $-0.1 \pm 0.2$ \\
$v \sin i_\text{rot}$\xspace\,(\mbox{km\,s$^{-1}$}\xspace) & $30.0\pm1.7$ & $17.1 \pm 2.0$ & $16.4 \pm 10.6$ & $22.2\pm 1.8$ \\
\hline
\end{tabular}}
\end{center}

\begin{flushleft}
$^{a}${Hubble guide star catalogue}\\
$^{b}${2MASS}\\
$^{c}${APASS Data Release 7, uncertainties are quoted where available as the scatter from multiple observations.}
\end{flushleft}
\end{table*}

To investigate the errors in our spectral typing pipeline, we observed seven reference stars from \citet{2005ApJS..159..141V}, and four known planet hosting stars of similar spectral type and brightness to our candidates \citep[WASP-61, 62, 78, 79][]{2012MNRAS.426..739H,2012A&A...547A..61S}. These observations were used to determine the echelle orders that yielded the most reliable spectral types. Reference stars with $v \sin i > 10\,\text{km}\,\text{s}^{-1}$ were also analysed at the finer 1\,\mbox{km\,s$^{-1}$}\xspace $v \sin i_\text{rot}$\xspace grid spacing. We are not sensitive to $v\sin i < 10\,$\mbox{km\,s$^{-1}$}\xspace rotational velocities, where we become limited by the instrument resolution. The RMS difference between our measured stellar parameters and literature values are 113\,K in \teff, 0.19\,dex in $\log g$\xspace, 0.12\,dex in [Fe/H]\xspace, and 4.4\,\mbox{km\,s$^{-1}$}\xspace in $v \sin i_\text{rot}$\xspace. After correcting for an empirical offset in each parameter, we get errors of 88\,K in \teff, 0.13\,dex in $\log g$\xspace, 0.09\,dex in [Fe/H]\xspace, and 0.7\,\mbox{km\,s$^{-1}$}\xspace in $v \sin i_\text{rot}$\xspace. The offsets have been incorporated in the stellar parameters presented here.

Macroturbulence and microturbulence are free parameters in 1D stellar atmosphere models that contribute to the overall broadening of the spectral features. We investigate the degeneracy between these parameters and the measured stellar rotational broadening. The spectrum of HATS550-016 was fitted to synthetic spectral grids generated at macro and microturbulences from 0 to 5\,\mbox{km\,s$^{-1}$}\xspace, producing a mean variation of 0.8\,\mbox{km\,s$^{-1}$}\xspace in the resulting $v \sin i_\text{rot}$\xspace measurement, smaller than our quoted measurement errors. Since the rotational broadening parameter for all host stars studied are much larger than the broadening from macro and microturbulence, we conclude minimal systematic uncertainty contributions from these parameters. In addition, we checked for the dependency of the measured $v \sin i_\text{rot}$\xspace to the synthetic spectral resolution, and found a variation of 0.6\,\mbox{km\,s$^{-1}$}\xspace over a change in resolution of 1000. Since the resolution is measured from the ThAr arc lamp spectra, we expect no significant contribution from uncertainties in the resolution to the $v \sin i_\text{rot}$\xspace systematic uncertainties.

\subsection{Global modelling of data}
\label{sec:lightcurve-analysis}

To derive the system properties, we performed simultaneous modelling of the HATSouth discovery photometry, follow-up photometry where available, and radial velocity measurements. The light curves were modelled using the \citet{1972ApJ...174..617N} model for eclipsing binaries, allowing for ellipsoidal phase variations, as implemented in the JKTEBOP code \citep{1981AJ.....86..102P,2004MNRAS.351.1277S}. The Keplerian orbit was used to model the radial velocity measurements.

The free parameters in the global fit include the orbital period $P$, transit time $T_0$, radius ratio $R_2/R_1$, normalised radius sum $R_\text{sum}=(R_1+R_2)/a$, radial velocity orbit semi-amplitude $K$, eccentricity parameters $e\cos\omega$ and $e\sin\omega$, and inclination $i$. Quadratic limb darkening coefficients for the primary star were fixed to values from \citet{2000A&A...363.1081C}. We assume uniform priors for all the free parameters. In the cases where the proposed iteration in inclination is $i>90^\circ$, we adopt the $180^\circ-i$ geometry to avoid the discontinuous boundary. To account for the non-zero flux contribution from the M-dwarf companion, we also obtained an approximate surface brightness estimate for the companion using a 5 Gyr \citet{1998A&A...337..403B} isochrone. However, the flux contribution from the M-dwarf is $\ll 0.1\text{\%}$ in the $R$ band and is negligible. Ellipsoidal variations are included in the model by including the mass ratio parameter $q$, using masses determined per iteration from isochrone fitting (see Section~\ref{sec:isochrone-fitting}). The best fitting parameters and the surrounding error space were explored by the \emph{emcee} \citep{2013PASP..125..306F} implementation of an Markov chain Monte Carlo (MCMC) ensemble sampler, with the individual measurement errors for all datasets (discovery, follow-up photometry, radial velocity) inflated such that the reduced $\chi ^2$\xspace is at unity.

Instrumental offsets were derived for each instrument separately. In addition, the HATSouth discovery light curves can be diluted in eclipse depth if they are treated by the TFA detrending algorithm. In the cases where well sampled follow-up photometry is available (HATS550-016 and HATS553-001), we fitted for a dilution factor for the HATSouth light curves, using the follow-up light curve as reference. Where follow-up photometry of the full transit is not available (HATS551-019 and HATS551-021), simultaneous TFA corrections were performed on the HATSouth light curve using the transit model for each MCMC iteration \citep[see Section 6,][]{2005MNRAS.356..557K}.

\subsection{Determination of mass and radius }
\label{sec:determ-mass-radi}

We derive the mass and radius of the primary and secondary stars at each iteration via 1) determination of the primary star properties from stellar isochrones using measured spectroscopic and light curve parameters, 2) assuming spin-orbit synchronisation for the system, and derive mass and radius from the spectroscopic $v \sin i_\text{rot}$\xspace measurement, and 3) a combined analysis that includes isochrone fitting and the assumption of spin-orbit synchronisation. Each analysis employs a separate MCMC routine that explores their respective posteriors.

\subsubsection{Isochrone fitting}
\label{sec:isochrone-fitting}
\citet{2007ApJ...664.1190S} showed that the normalised orbital distance $a/R_1$, derived from the global fit, can be combined with model isochrones to refine the stellar atmosphere parameters. $a/R_1$ is related to the mean stellar density by
\begin{equation}
  \label{eq:aRs_eq}
  \frac{M_1}{R_1^3} = \frac{4\pi^2}{G P^2} \left(\frac{a}{R_1} \right)^3 - \frac{M_2}{R_1^3} \, .
\end{equation}
Although the second term is usually insignificant and often discarded in the case of transiting planets, it cannot be ignored for stellar mass companions \citep{2013Aamp;A...549A..18T}. Therefore, for each iteration of the minimisation and MCMC routines, we used initial estimates of $M_1$ and $R_1$ to derive $M_2$ from the radial velocity orbit, then used the $M_2$ estimate and the fitted $a/R_1$, and spectroscopically determined \teff and [Fe/H]\xspace to derive new theoretical $M_1$ and $R_1$ values by isochrone fitting. Finally, the new primary mass and radius were used to derive a refined $M_2$ estimate. The Yonsei-Yale isochrones \citep{2001ApJS..136..417Y} provide the theoretical stellar masses and radii. To incorporate the uncertainties in the spectroscopic stellar parameters into the error analysis, \teff and [Fe/H]\xspace were drawn from Gaussian distributions in the MCMC routine. This method also gives us a more precise estimate for $\log g$\xspace of the primary star. This $\log g$\xspace value was incorporated into the spectral classifications process (Section~\ref{sec:host-star-properties}) to better constrain the \teff, [Fe/H]\xspace, and $v \sin i_\text{rot}$\xspace estimates.

\subsubsection{Spin-orbit synchronisation}
\label{sec:spin-orbit-synchr}
For stellar mass binaries at short periods, spin-orbit synchronisation via tidal interactions is expected to occur within $\sim 100$\,Myr \citep{1977A&A....57..383Z,1981A&A....99..126H}. If we assume spin-orbit synchronisation for these systems, and that the stellar spin-axis is near-perpendicular to our line-of-sight $(i_\text{orb} = i_\text{rot})$, then it is also possible to derive model-independent estimates of the stellar masses and radii \citep[e.g.][]{2007ApJ...663..573B}. The masses and radii of components A and B can be calculated from purely observable quantities using:
\begin{align}
  \label{eq:sync-mass-radius}
  M_1 &= \frac{P}{2\pi G} \left(\frac{a}{R_1}\right)^2 (v\sin i_\text{rot})^2 \\ & \times \left[ \frac{(a/R_1) v \sin i_\text{rot} - K\sqrt{1-e^2}}{\sin^3 i_\text{orb}} \right] \nonumber \\
  M_2 &= \frac{P}{2\pi G}  \left(\frac{a}{R_1}\right)^2 \left[ \frac{K (v\sin i_\text{rot})^2 \sqrt{1-e^2}}{\sin^3 i_\text{orb}} \right] \\
  R_1 &= \frac{P}{2\pi} \frac{v \sin i_\text{rot}}{\sin i_\text{orb}} \\
  R_2 &= R_1 \left(\frac{R_2}{R_1}\right) \,.
\end{align}

We caution that spin-orbit synchronisation and the alignment of the stellar spin-axis should not be automatically assumed. Although rapid synchronisation is expected for binary systems, some previous F-M binaries have been measured to be asynchronous \citep[e.g.][]{2005A&A...433L..21P,2006A&A...447.1035P,2013Aamp;A...549A..18T}. In addition, whilst the alignment of the stellar spin and companion orbital axes is also often predicted from formation and tidal interactions, (and by extension of the transit geometry the stellar spin-axis should also be perpendicular to our line-of-sight) spin-orbit misaligned stellar binaries have been identified \citep[DI Her, KOI-368,][]{2009Natur.461..373A,2013ApJ...776L..35Z}. It is therefore necessary to compare the stellar parameter results from synchronisation against that of isochrone fitting before this method can be adopted.

For each iteration of the global minimisation and MCMC routine, we also calculated the primary and companion masses and radii assuming synchronisation. The adopted $v \sin i_\text{rot}$\xspace value was given by the spectroscopic analysis, and was drawn from a Gaussian distribution in the MCMC error analysis.

\subsubsection{Combined mass-radius estimate}
\label{sec:combined-mass-radius}

We also perform a combined analysis, where the mass and radius are calculated using isochrone fitting as described in Section~\ref{sec:isochrone-fitting}. The expected $v \sin i_\text{rot}$\xspace is then derived using the period and radius, and compared to the measured $v \sin i_\text{rot}$\xspace. We calculate an additional $\chi ^2$\xspace term,
\begin{equation}
  \label{eq:chisq-vsini}
  \chi^2_{v\sin i_\text{rot}} = \left(\frac{2\pi R_1 \sin i_\text{orb}/P - v \sin i_\text{rot}}{\Delta v \sin i_\text{rot}}\right)^2 \, ,
\end{equation}
which is added to the $\chi ^2$\xspace from the light curve and radial velocity data. Due to the transit geometry, we approximate $\sin i_\text{orb}\approx 1$ in the calculation. The MCMC minimisation is re-run for this combined analysis.\\

The probability distributions for the mass and radius, measured using the above techniques, are plotted in Figure~\ref{fig:posterior}. We find that the $2\sigma$ confidence regions derived using isochrone and synchronisation overlap for all the systems. This indicates that the assumption of spin-orbit synchronisation, required for the combined analysis (Section~\ref{sec:combined-mass-radius}), is valid for all systems. The system parameters from the combined analysis is adopted for discussion here onwards. The stellar and system parameters are presented in Table~\ref{tab:stellar-params}.

\input{params_table.tex}

\input{system_plots.tex}

\begin{figure*}
  \centering

  \begin{tabular}{cc}
      \includegraphics[width=9cm]{plots/posterior_HATS550-016.eps}&
      \includegraphics[width=9cm]{plots/posterior_HATS551-019.eps}\\
      \includegraphics[width=9cm]{plots/posterior_HATS551-021.eps}&
      \includegraphics[width=9cm]{plots/posterior_HATS553-001.eps}\\
  \end{tabular}
  \caption{The 1 and 2$\sigma$ confidence regions for the masses and radii of the VLMS systems presented in this study. We plot individual confidence regions derived from the isochrone fit (blue), assuming spin-orbit synchronisation (red), and the combined analysis (gray). The confidence regions from the combined analysis is adopted. The corresponding crosses mark the peak of the probability distributions.}
  \label{fig:posterior}
\end{figure*}

We also tested the sensitivity of the final results against various assumptions in the methods outlined above. These tests were performed on the HATS550-016 dataset. The limb darkening coefficients were set free and allowed to vary within 0.2 of the values from \citet{2000A&A...363.1081C}. The resulting system parameters did not deviate from those presented in Table~\ref{tab:stellar-params}, with no significant increase in the uncertainties. To test the dependence of the results on the Yonsei-Yale isochrones, we performed the analysis in Section~\ref{sec:isochrone-fitting} using the Dartmouth isochrones \citep{2008ApJS..178...89D}, but found no deviation in the results. To test the effectiveness of reconstructive TFA  \citep{2005MNRAS.356..557K} at recovering the true transit shape, we analysed the HATS550-016 system using only the HATSouth discovery data by excluding the follow-up photometry observations, and found no significant deviation in the results, however the uncertainties were increased by a factor of $\sim2-3$. We caution that correlated noise, present in the follow-up light curve, were unaccounted for in the analysis, and may lead to under-estimated uncertainties.

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

We have presented the discovery of four transiting VLMSs, with masses ranging from 0.1 to 0.2\,$M_\odot$. Their properties are discussed briefly below.

\subsection{HATS550-016B}
\label{sec:hats550-016b}

HATS550-016B is the lowest mass star within our sample, and is the second lowest mass star known with mass and radius determined to better than $10\text{\%}$ \citep[after J1219-39b;][]{2013Aamp;A...549A..18T}. It has a mass and radius of $0.110_{-0.006}^{+0.005}\, M_\odot$ and $0.147_{-0.004}^{+0.003}\,R_\odot$, and orbits a relatively metal deficient $(\text{[Fe/H]}=-0.60\pm0.06)$ F type star of age $5_{-1}^{+3}$ Gyr in a period of $2.051811_{-0.000002}^{+0.000002}$ days. The radius of HATS550-016B is inflated by 13\% compared to \citet{1998A&A...337..403B} models, assuming it has the same metallicity as the primary star. It is the only star in this sample that is inflated with respect to the isochrones.

\subsection{HATS551-019B}
\label{sec:hats551-019b}

HATS551-019B is a $0.17_{-0.01}^{+0.01}\,M_\odot$ , $0.18_{-0.01}^{+0.01}\,R_\odot$ VLMS with a $4.68681_{-0.00001}^{+0.00002}$ day period orbit a $6_{-2}^{+2}$ Gyr F subgiant, with sub-solar metallicity of $\text{[Fe/H]} = -0.4\pm 0.1$. Since the follow-up photometry of HATS551-019 covers only the egress event, the HATSouth discovery light curves, detrended using simultaneous TFA, are also used to constrain the $R_2/R_1$ ratio. The radius of HATS551-019B agrees with theoretical predictions to within errors.

\subsection{HATS551-021B}
\label{sec:hats551-021b}

HATS551-021B is a $0.132_{-0.005}^{+0.014}\,M_\odot$, $0.154_{-0.008}^{+0.006}\,R_\odot$ VLMS in a $3.63637_{-0.00005}^{+0.00005}$ day period orbit about an F dwarf with metallicity of $\text{[Fe/H]} = -0.4\pm0.1$. The age of the primary star is ill defined from isochrone fitting ($4_{-4}^{+3}$ Gyr). We find no chromospheric Ca HK emission, nor excess Li absorption, indicating that the system is likely $>1$ Gyr in age. No follow-up photometry is available for HATS551-021, so the $R_2/R_1$ ratio is constrained purely from HATSouth discovery light curves. The radius of HATS551-021B matches theoretical isochrones very well.

\subsection{HATS553-001B}
\label{sec:hats553-001b}

HATS553-001B is a VLMS with mass of $0.20_{-0.02}^{+0.01}\,M_\odot$, and radius of $0.22_{-0.01}^{+0.01}\,R_\odot$, orbiting a $3_{-2}^{+2}$ Gyr F type star of near solar metallicity $(\text{[Fe/H]} = -0.1\pm0.2)$ in a $3.80405_{-0.00001}^{+0.00001}$ day period orbit. The radius of HATS553-001B matches the isochrones to within errors.

\subsection{Mass--radius relationship}
\label{sec:mass-radi-relat}

The masses and radii of the VLMS companions presented in this paper, as well as that of known well-studied VLMSs (Table~\ref{tab:prev_stars}) are plotted in Figure~\ref{fig:mass_radius}. Of the VLMSs reported in this study, we find only HATS550-016B to be inflated compared to theoretical isochrones, HATS551-019B, HATS551-021B, and HATS553-001B agree with the isochrone mass-radius relations to within measurement uncertainties.

\begin{figure*}
  \centering
  \includegraphics[width=15cm]{plots/mass_radius_best.eps}
  \caption{Mass--radius diagram of the VLMSs. New VLMSs presented in this paper are plotted in red and labelled, known F,G-M eclipsing binaries are plotted as cyan squares, M-M eclipsing binaries as magenta circles, and single stars measured by interferometry as blue crosses (Table~\ref{tab:prev_stars}). Isochrone lines from \citet{1998A&A...337..403B} at 1.0 Gyr solar (black dashed), 5.0 Gyr solar (black solid), 5.0 Gyr $\text{[M/H]}=-0.5$ (black dotted), and from \citet{2008ApJS..178...89D} at 5.0 Gyr solar (green solid), 5.0 Gyr $\text{[M/H]}=-0.5$ (green dotted)  are marked. The corresponding 1 and 5 Gyr isochrones for brown dwarfs from \citet{2003A&A...402..701B} are plotted in black, but not used in further analysis.}
  \label{fig:mass_radius}
\end{figure*}

We tested for any general radius deviation between the observed VLMS population and the isochrones. The theoretical radii are taken from the 5 Gyr isochrones from \citet{1998A&A...337..403B}, interpolated between $\text{[M/H]}=-0.5$ and 0.0, and linearly extrapolated beyond when necessary, to account for the metallicity dependency. For each object, we sample the isochrones via a Monte Carlo analysis, drawing mass and metallicity values from Gaussian distributions about the measured values and their associated uncertainties, and derive a predicted model radius and uncertainty. For this discussion on the radius deviation between model and measurements, we adopted the radius uncertainty as the quadrature addition of the uncertainties in the measurement and model sampling.

We also note that the difference between the \citet{1998A&A...337..403B} and the Dartmouth isochrones \citep{2008ApJS..178...89D} is minor compared to the deviation from observations (see green isochrone lines in Figure~\ref{fig:mass_radius}), hence the following calculations were performed relative to the \citet{1998A&A...337..403B} isochrones only. In addition, we also explored isochrones of younger ages and shorter mixing length using the \citet{1998A&A...337..403B} isochrones, neither factors have obvious effects at this mass range.

The $\chi ^2$\xspace of the observed population is compared to (Model A) the isochrones without modification and (Model B) with isochrone radii inflated by 1.05. If the $\chi ^2$\xspace is calculated with the measurement uncertainties taken at face value, the Bayesean Information Criterion (BIC) between the two models is 50 ($\chi^2/\text{dof} = 7$ and 3, for Models A and B respectively), tentatively favouring an inflation of radius from the isochrones. The F-test for the variance ratio of the fit to the two models gives a p-value of 0.08, suggesting a very tentative preference towards Model B. Both BIC and the F-test account for the greater complexity of Model B over A. A number of studies \citep{2010ApJ...712.1003W,2010ApJ...718..502M,2012ApJ...757...42F} have commented that the presence of spots can impose radii uncertainties on the order of 2\% in these measurements. After imposing a minimum radius uncertainty of 2\% on the same population, we find $\text{BIC}=21$ ($\chi^2/\text{dof}=3$ and 2, for Models A and B respectively) and F-test p-value of 0.11. The F-test result, after inflating the uncertainties, suggests no real preference between Models A and B. In addition, 5\% systematic deviation between measurements and model is significantly smaller than the $\sim10$\% stated by earlier studies \citep[e.g.][]{2006Ap&SS.304...89R}, and agrees with more recent studies of higher mass double-lined M-dwarf binaries, using newer isochrone sets \citep[e.g.][]{2011ApJ...728...48K,2012ApJ...757...42F,2013ApJ...776...87S}.

The RMS scatter of $\text{observed}-\text{theoretical}$ stellar radius difference (3\%) is slightly larger than the mean observational uncertainties (5\%). Whilst this is likely due to the under-estimated observational uncertainties, it may also point towards secondary factors, beyond mass and metallicity, that affect the radii of VLMSs. Figure~\ref{fig:MR-trends} plots the radius discrepancy against mass, orbital period, and incident flux from the primary star. For each factor, the Pearson correlation coefficient $r$ is calculated, weighted by the measurement uncertainties, with the radius uncertainties of M-M binaries increased to 2\%. We find no significant correlation with any of these parameters.

\begin{figure}
  \centering
  \includegraphics[width=9cm]{plots/MR-trends.eps}
  \caption{The $\text{observed}-\text{theoretical}$ radius difference of the VLMSs are plotted against their (a) mass, (b) system period, and (c) incident flux from the primary star. The theoretical radius is derived from the \citet{1998A&A...337..403B} isochrones, interpolated to the [Fe/H] of each system. Objects without relevant orbital period and host star flux are omitted where necessary. Panel (d) shows the radius deviation to a solar metallicity isochrone as a function of the measured metallicity. The Pearson correlation coefficient $r$ is calculate for each panel. We find no significant correlation between the radius discrepancy and any of these parameters.}
  \label{fig:MR-trends}
\end{figure}

In particular, activity induced inflation of the stellar radius should be correlated with shorter period if faster rotation gives rise to more powerful internal dynamos \citep{2007ApJ...660..732L}. This is not observed in the low mass population. However, it is not obvious that we expect such period-activity-radius dependencies, since the dynamos in fully convective stars may operate differently to solar type stars \citep{2006A&A...446.1027C}. In addition, the paucity of well studied VLMS binaries in $>$10 day periods prevent us from drawing strong conclusions regarding the period--radius dependency. We also note the minimal dependency between incident flux and radius deviation. The influence of irradiation and disequilibrium chemistry on exoplanets has been contemplated \citep[e.g.][]{2010ApJ...720.1569K}, similar mechanisms that alter the top-level opacity of VLMSs may be possible, but clearly are not significant. In addition, whilst external influences are often considered when discussing the radius discrepancy of binary systems, we note that field M-dwarfs measured via interferometry have shown an equivalent radius discrepancy to the models \citep[e.g.][]{2006ApJ...644..475B,2012ApJ...757..112B,2013ApJ...776...87S}, and that there is no necessary expectation for radius, period, and incident flux to be correlated.

Metallicity has previously been suggested as a cause in the radius discrepancy \citep[e.g.][]{2006ApJ...644..475B,2011ApJ...736...47B}. Figure~\ref{fig:MR-trends} also plots the radius deviation to the solar metallicity isochrone. We find no correlation between the measured metallicity and the radius deviation. The lack of dependancy on metallicity for VLMSs agrees with the analysis by \citet{2013ApJ...776...87S}, who suggests that metallicity is only weakly correlated with radius, but more strongly affects luminosity and effective temperature.

\input{literature_values.tex}

\section*{Acknowledgments}

Development of the HATSouth project was funded by NSF MRI grant
NSF/AST-0723074, operations are supported by NASA grant NNX09AB29G, and
follow-up observations receive partial support from grant
NSF/AST-1108686.
Work at the Australian National University is supported by ARC Laureate
Fellowship Grant FL0992131.
Followup observations with the ESO~2.2\,m/FEROS instrument were
performed under MPI guaranteed time (P087.A-9014(A), P088.A-9008(A),
P089.A-9008(A)).
AJ acknowledges support from FONDECYT project 1130857, BASAL CATA
PFB-06, and the Millenium Science Initiative, Chilean Ministry of
Economy (Nuclei: P10-022-F, P07-021-F).
RB and NE are supported by CONICYT-PCHA/Doctorado Nacional and MR
is supported by FONDECYT postdoctoral fellowship 3120097.
This work is based on observations made with ESO Telescopes at the La
Silla Observatory under programme IDs P087.A-9014(A), P088.A-9008(A),
P089.A-9008(A), P087.C-0508(A), 089.A-9006(A), and
This paper also uses observations obtained with facilities of the Las
Cumbres Observatory Global Telescope.
We acknowledge the use of the AAVSO Photometric All-Sky Survey (APASS),
funded by the Robert Martin Ayers Sciences Fund, and the SIMBAD
database, operated at CDS, Strasbourg, France.
Operations at the MPG/ESO 2.2\,m Telescope are jointly performed by the
Max Planck Gesellschaft and the European Southern Observatory.  The
imaging system GROND has been built by the high-energy group of MPE in
collaboration with the LSW Tautenburg and ESO \citep{2008PASP..120..405G}.  We thank Timo Anguita
and R\'egis Lachaume for their technical assistance during the
observations at the MPG/ESO 2.2\,m Telescope.
GZ thanks helpful discussions and draft proof readings by C.X. Huang.
\bibliographystyle{mn2e}

redpajama_set_name: RedPajamaArXiv


They say memories are golden, well maybe that is true.
I never wanted memories, I only wanted you.
I loved Hector with all my heart and soul. He was an amazing man. What I felt for Hector, how he made me feel and how I am feeling now that he has gone is hard to explain, but these song go part way there.


SweClockers redaktion fattar kaffemuggarna i ett fast grepp, och lotsar vilsna lyssnare genom djungeln av tekniknyheter.
In this series of podcasts Vasilis van Gemert asks various digital designers what makes a digital thing good, and what bad. It is a question about quality, and its many definitions. Definitions that will often conflict. Most — but not all — episodes will be in Dutch.


text:
package com.blankj.androidutilcode.main;

import android.graphics.Color;
import android.os.Bundle;
import android.support.design.widget.CollapsingToolbarLayout;
import android.support.v7.app.ActionBarDrawerToggle;
import android.support.v7.widget.Toolbar;
import android.view.View;

import com.blankj.androidutilcode.R;
import com.blankj.androidutilcode.base.BaseDrawerActivity;
import com.blankj.androidutilcode.core.main.CoreUtilActivity;
import com.blankj.androidutilcode.sub.main.SubUtilActivity;
import com.blankj.utilcode.util.BarUtils;

/**
 * <pre>
 *     author: Blankj
 *     blog  : http://blankj.com
 *     time  : 2016/09/29
 *     desc  : MainActivity
 * </pre>
 */
public class MainActivity extends BaseDrawerActivity {

    @Override
    public void initData(Bundle bundle) {

    }

    @Override
    public int bindLayout() {
        return R.layout.activity_main;
    }

    @Override
    public void initView(Bundle savedInstanceState, View view) {
        Toolbar toolbar = (Toolbar) findViewById(R.id.toolbar);
        View fakeStatusBar = findViewById(R.id.fake_status_bar);
        CollapsingToolbarLayout ctl = (CollapsingToolbarLayout) findViewById(R.id.ctl);
        ctl.setExpandedTitleColor(Color.parseColor("#00FFFFFF"));
        setSupportActionBar(toolbar);
        ActionBarDrawerToggle toggle = new ActionBarDrawerToggle(this,
                rootLayout,
                toolbar,
                R.string.navigation_drawer_open,
                R.string.navigation_drawer_close);
        rootLayout.addDrawerListener(toggle);
        toggle.syncState();

        BarUtils.setStatusBarAlpha4Drawer(this, rootLayout, fakeStatusBar, 0, false);
        BarUtils.addMarginTopEqualStatusBarHeight(toolbar);
    }

    @Override
    public void doBusiness() {

    }

    @Override
    public void onWidgetClick(View view) {

    }

    public void coreUtilClick(View view) {
        CoreUtilActivity.start(this);
    }

    public void subUtilClick(View view) {
        SubUtilActivity.start(this);
    }
}

redpajama_set_name: RedPajamaGithub


Does anyone have any ideas on entering "Tasks" to preventative work orders? I know that I can enter them line by line under the Tasks and Procedures section, but that would be very time consuming. I wanted to attach a writable PDF but the application will not allow it.
Has anybody done anything different?


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text:
William "Bill" James Pines
William "Bill" James Pines, age 86, of Greensboro, passed away Wednesday November 17, 2021. A funeral service will be held 2:00 PM Sunday November 21, 2021 at Temple Emanuel on Jefferson Rd. Interment will follow at the Hebrew Cemetery. Bill Pines was born in Tulsa OK on November 12, 1935 to the late Muriel and Harry Pines. At the age of 2 the family moved to Los Angeles, CA. He treasured memories of golf at Rancho Park and friends from Hamilton High. To fulfill his duty to country, he joined the Army Reserves and was honorably discharged at the rank of Sargent after 6 years of summer camps. After graduating from UCLA Bill went to work selling fabrics in the L.A. area. He married Miriam "Midge" Heymann in 1965 and they had 2 boys. Bill learned that North Carolina was the place to sell fabric - he made a sales trip to High Point and called Midge saying "It's beautiful here, pack up, we're moving, so in 1969 they moved to Greensboro NC. where they made many friends, who became family to them, sharing holidays, and joy and sorrows of life. Bill was an independent contractor who sold for Dorell, David and Dash, JB Martin and Weave Corporation. His employers and customers were very important to him – he was respected, loyal, always honest, patient and proud of their success. Bill enjoyed his job as if he were going to a party everyday. His career started from being the "kid" on the block to "The Dean". Bill loved mentoring "Kids" to become good salesmen. As important as his career was to him, Bill's family and friends had his full attention. Bill is survived by his loving wife Miriam "Midge" Heymann, sons Nicholas Edward Pines and wife Rhonda Teague, Harold Russell Pines and wife Kathleen Pines, and Benjamin Stuart Pines and wife Patricia Gladden Pines, brother, Michael Pines, sister Margot (Pines) Moore, and grandchildren Hannah Eve Pines, Avery Elizabeth Pines, and Kinsey Muriel Pines. In lieu of flowers, memorials may be made to Temple Emanuel Chesed committee or choose any of the many charities that feed the hungry. Online condolences at www.forbisanddick.com.
William "Bill" James Pines, age 86, of Greensboro, passed away Wednesday November 17, 2021. A funeral service will be held 2:00 PM Sunday November 21, 2021 at Temple Emanuel on Jefferson Rd. Interment will follow at the Hebrew Cemetery. Bill... View Obituary & Service Information
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redpajama_set_name: RedPajamaCommonCrawl


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Direct log-in
+994 12 493 14 14 | *0808
Hotline from Azerbaijan
Ticket Refund and Exchange
Fares and Services
Onboard Meals
Priority Seats
Note for Transfer Passengers
For passengers travelling to Turkey
For passengers Travelling to/from EU
Baku, Heydar Aliyev
Gandja
Tehran, Imam Khomeini
Moscow, Vnukovo
Alanya , Gazipasa
Ankara, Esenboga
Istanbul, S.Gokcen
Kiev, Borispol
Kiev, Zhuliany
(2 to 11 years)
Infants: 0
(up to 2 years)
Where do you want to go? Antalya, Turkey Baku, Azerbaijan Gabala, Azerbaijan Gandja, Azerbaijan Istanbul, Turkey Kazan, Russia Kiev, Ukraine Lviv, Ukraine Mineralnye Vody, Russia Moscow, Russia St Petersburg, Russia Tbilisi, Georgia Tehran, Iran
Age of child(ren) 1 2 3 4 5 6 7 8 9 10 11 12 13 14 15 16 17
Pick-up location Alanya , Turkey, Gazipasa (GZP) Ankara, Turkey, Esenboga (ESB) Astrakhan, Russia, (ASF) Bahrain, Bahrain, (BAH) Baku, Azerbaijan, Heydar Aliyev (GYD) Batumi, Georgia, (BUS) Dammam, Saudi Arabia, (DMM) Gandja, Azerbaijan, (KVD) Istanbul, Turkey, S.Gokcen (SAW) Izmir, Turkey, (ADB) Kazan, Russia, (KZN) Kharkiv, Ukraine, (HRK) Kiev, Ukraine, Borispol (KBP) Kiev, Ukraine, Zhuliany (IEV) Lviv, Ukraine, (LWO) Mineralnye Vody, Russia, (MRV) Moscow, Russia, Vnukovo (VKO) Odesa, Ukraine, (ODS) Riyadh, Saudi Arabia, (RUH) St Petersburg, Russia, (LED) Tbilisi, Georgia, (TBS) Tehran, Iran, Imam Khomeini (IKA) Ufa, Russia, (UFA)
Drop-off location Alanya , Turkey, Gazipasa (GZP) Ankara, Turkey, Esenboga (ESB) Astrakhan, Russia, (ASF) Bahrain, Bahrain, (BAH) Baku, Azerbaijan, Heydar Aliyev (GYD) Batumi, Georgia, (BUS) Dammam, Saudi Arabia, (DMM) Gandja, Azerbaijan, (KVD) Istanbul, Turkey, S.Gokcen (SAW) Izmir, Turkey, (ADB) Kazan, Russia, (KZN) Kharkiv, Ukraine, (HRK) Kiev, Ukraine, Borispol (KBP) Kiev, Ukraine, Zhuliany (IEV) Lviv, Ukraine, (LWO) Mineralnye Vody, Russia, (MRV) Moscow, Russia, Vnukovo (VKO) Odesa, Ukraine, (ODS) Riyadh, Saudi Arabia, (RUH) St Petersburg, Russia, (LED) Tbilisi, Georgia, (TBS) Tehran, Iran, Imam Khomeini (IKA) Ufa, Russia, (UFA)
Driver age 18 19 20 21 22 23 24 25 26 27 28 29 30 31 32 33 34 35 36 37 38 39 40 41 42 43 44 45 46 47 48 49 50 51 52 53 54 55 56 57 58 59 60 61 62 63 64 65 66 67 68 69 70 71 72 73 74 75 76 77 78 79 80 81 82 83 84 85 86 87 88 89 90 91 92 93 94 95 96 97 98 99
Buta Airways replenished its fleet with new Embraer E-190
September 18 2018, Baku – Azerbaijan's low-cost airline Buta Airways received a new Embraer E-190, which was delivered to the airline's fleet directly from the manufacturer in Brazil.
It is the seventh in the low-cost airline's fleet and will allow add more flights to the most popular destinations in the airline's flight schedule.
The new aircraft of Buta Airways is named after the Nakhchivan Autonomous Republic's Gunnut village, which was recently liberated from Armenian occupation.
By tradition, the new aircraft was welcomed at the Heydar Aliyev International Airport with a water salute. Special guest of the welcoming ceremony was a resident of the liberated Gunnut village.
You can watch the video of Günnüt aircraft welcoming ceremony on the following link:
https://youtu.be/2BbBLLSVMy8
It should be noted that in the near future it is expected to replenish the fleet of Buta Airways with another new aircraft of this type. Replenishment of the fleet with the new aircraft will expand the airline's route network.
Buta Airways is the first low-cost airline in Azerbaijan, a structural unit of the CJSC Azerbaijan Airlines (AZAL). It was founded in December 2016. The first flight was carried out on September 1, 2017. The Airline's fleet consists of modern Embraer E-190 aircrafts.
The Airline is based in Baku, at the Heydar Aliyev International Airport and carries out flights to the most popular destinations.
You can follow all updates and news on the social networks pages of Buta Airways:
facebook.com/ButaAirways
instagram.com/ButaAirways
twitter.com/ButaAirways
t.me/Buta_Airways
Press service of Buta Airways
Low-cost airline Buta Airways launches direct flights to Lviv
Buta Airways flights to Kyiv from January 22, 2020 will be operated to Boryspil airport
Buta Airways will launch flights to new destinations in the Middle East
© 2019 Buta Airways
Trademark of Azerbaijan Airlines CJSC
*0808 Hotline from Azerbaijan
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Number of infants may not exceed number of adults travelling with them. For booking with more than 1 infant (age 0-2 year) please contact our Call Center +99412 493 14 14 callcenter@butaairways.az
Booking engine is temporarily unavailable due to the site upgrade.
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We are an Authorized MTD Dealer carrying a large selection of MTD Springs.
If you do not see the MTD Spring you need, please complete the Lawn Mower Parts Request Form and we will be happy to assist you.
Contains service part number 490179.


With so many things to do in Kingscliff, it's important to choose a good Hotel.
Located opposite to the beach, the Paradiso Resort Kingscliff is in the Northern New South Wales and is 25 kilometres from the airport. The Tropical Fruit World, Mt Warning National Park as well as the theme parks of the Gold Coast are the major attractions in Kingscliff.


Oak Bay is a visually stunning district on the southern tip of Vancouver. There are three golf courses and more than 20 charming restaurants and cafes in Oak Bay. Families can enjoy a dip in the pool which is open until 1 a.m. or feed seals or otters by the dock. Old Bay's Willows Beach is an ideal getaway during winter and summer. The area also boasts a variety of art galleries on Old Bay Avenue.
With waterfront, restaurants, parks and festivals, Old Bay is a perfectly melded combination of soothing nature and bustling social activity.


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import { Type } from './abstract';
export declare class IntersectionType extends Type {
    types: Type[];
    readonly type: string;
    constructor(types: Type[]);
    clone(): Type;
    equals(type: IntersectionType): boolean;
    toObject(): any;
    toString(): string;
}


— Chris Wallace on Sunday, May 15th, 2016 in an episode of "Fox News Sunday"
By Lauren Carroll on Wednesday, May 18th, 2016 at 10:30 a.m.
The presumptive Republican nominee for president has refused to release his tax returns thus far, citing an IRS audit. Presidential candidates are not required to release tax returns, but the information helps the public vet a candidate's finances, revealing information such as charitable giving, investments and the tax rate he pays.
The IRS has said recently that an audit does not bar a person from releasing their own tax information.
On the Democratic side of the race, Sen. Bernie Sanders has released his 2014 returns, and former Secretary of State Hillary Clinton has released annual returns going back to 2000.
In a May 15 interview with Republican National Committee Chair Reince Priebus, Fox News Sunday host Chris Wallace noted that it's become customary over the past several decades for presidential candidates to release their tax returns.
"He says that he's not going to release them until an IRS audit is complete," Wallace said, speaking of Trump. "He was asked this week what his effective tax rate is, he said it's none of your business. Look, you know, you talk about this, but every Republican nominee since Richard Nixon, who at one time was under an audit, has released their tax returns."
Noting that it was "not good" that Mitt Romney stalled on releasing his tax returns in the 2012 race, Priebus said, "I'm not sure whether Americans actually care or not whether Donald Trump releases his taxes or not."
We've looked into the history of candidate tax returns before. But we haven't dug into the story of former President Richard Nixon's audit, so we thought we should put Wallace's claim on the Truth-O-Meter.
The Tax History Project has compiled the tax returns of many current and former candidates and presidents, all the way back to Franklin Roosevelt's 1913 returns.
Each Republican nominee in the past nine presidential elections has released his tax returns: Ronald Reagan (1980, 1984), George H. W. Bush (1988, 1992), Bob Dole (1996), George W. Bush (2000, 2004), John McCain (2008) and Mitt Romney (2012).
That leaves one nominee since Nixon, Nixon's vice president, Gerald Ford. Ford assumed the role of president after Nixon resigned in 1974 amid the Watergate scandal. Ford ran for re-election as the Republican nominee in 1976, ultimately losing to Democrat Jimmy Carter.
Ford never released his full tax returns. He released summary data about his returns from 1966 through 1974. The summary data includes his total income and the total tax he paid but not an itemized breakdown.
Back to Nixon. Nixon did not release his tax returns in 1968 or 1972.
However, the congressional investigation ultimately found that Nixon owed $476,431 (approximately $2.3 million in today's dollars) in unpaid taxes and accrued interest. Oops.
We asked Joe Thorndike, director of the Tax History Project, if the IRS has audited any presidents or presidential candidates since Nixon. He said he doesn't know — and it would be impossible to know unless the auditee volunteered that information because the IRS can't confirm or deny anything about a particular taxpayer.
Thorndike added, though, that he thinks it's likely the IRS has audited candidates and presidents in recent years.
Wallace said, "Every Republican nominee since Richard Nixon, who at one time was under an audit, has released their tax returns."
Wallace's telling of history is a little off, though the force of his point is correct: The Republican has released his tax returns in the last nine presidential cycles. We rate this claim Mostly True.
Published: Wednesday, May 18th, 2016 at 10:30 a.m.


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Nereśl – rzeka, prawy dopływ Narwi o długości 45,13 km.

Płynie w powiecie monieckim w województwie podlaskim. Przepływa przez jezioro Zygmunta Augusta.

Zobacz też
 Rzeki Polski

Przypisy

Bibliografia

Dorzecze Narwi

redpajama_set_name: RedPajamaWikipedia


It's that time of every four years again, the Super Bowl of American Marathoning, the Olympic Trials. Daily Relay will be previewing the race all week and will have onsite coverage all weekend. Yesterday, we gave our Women's picks. Today, we give our picks for the Men's race.
If you're doubting Rupp, my response is C'mon, man. At anything short of a marathon, he's so much better than anyone else in the race that I'm willing to ignore the fact that it's his first time. Lots can go wrong in 26.2 miles, so he's not a lock, but this is a great way to break into the distance: unlike a big international race, he doesn't have to chase any 2:04-types. Only two men in this race have ever broken 2:10 and both are on the downside of their careers.
I have stopped deciding he can't do things. Long ago I thought his career was shot, that he belonged on the scrapheap, and I was so wrong. He's not stupid enough to think he has to win this, he knows that third is as good as first at the Trials. He is the Master Po in this race and has plenty of patience.
At his best, Ritz was as good or better a marathoner than anyone in this field, Rupp included. While those days are three or four years in the past, it sounds like he's put together an extended period of injury-free running, and anytime he's done that he's been en fuego.
This will be his fourth career marathon and his progression has been 2:16:44 to 2:13:24 to 2:11:20. Coach Kevin Hanson thinks he's ready to make another jump in performance.
Why: Even though he is 40, he has the least amount of question marks of any of the top runners. He ran well in New York in November and is perfectly suited for the championship style race.
Why Not: Eventually he has to slow down and he has had bad races in the past where he finishes off the pace. Those races, however, are vastly outnumbered by the ones where he exceeds expectations.
Why: There aren't many people on the start line who have run 2:10, put up a great tune-up race and are in the upswing of their career. Puskedra can claim all three.
Why Not: It's his first attempt at the Olympic Marathon Trials. Patience will be important especially if the pace is slow in the early miles.
Why: He wouldn't race it if he wasn't ready and if he's ready then it's going to be fast. His half-marathon in December was effortless. On personal bests and talent, Rupp is on another level than everyone else in the field.
Why Not: There is no guarantee with marathon debuts. While the championship style race is slower than a rabbited major marathon, it's also more unpredictable. The fluctuations in pace could cause some problems for a first timer.
Why: Debuted with a 2:11:31 in Chicago last year. Can he do even better on his second try?
Why Not: This is a different style race than Chicago and he will more than likely have to improve on his great debut to finish in the top three.
Why: He appears to have had a good buildup. He has the fastest PR in the field and is still within his prime (though towards the end of it). He finished well ahead of Meb in Boston last April.
Why Not: If he's healthy, he's going to be hard to beat on the men's side. But he's not always healthy.
Why: He's consistent; he appears to have had a good buildup; he seems to always come through when it counts. This is a good but not great field. There are enough people in it who could beat him on an off day, but who really expects Meb to have an off day?
Why Not: He's shown signs of age in his last couple of marathons, including Boston in the spring and New York in the fall. He may not have another good marathon left in his legs.
Why: He's the most talented distance runner in America. He wouldn't have hopped in this race without appropriate planning and preparation. No one in this field can touch him in the 5K or 10K. The men's field is deep but not top-heavy.
Why Not: First marathon; weird buildup — inexperience proves too much to overcome or he just doesn't have it left in his legs the last 5K. The most likely scenario for him not making the team is a too-fast first 30K. It's hard to imagine him not finishing top three off a slow pace.
Why: Bruce has a pedigree of winning lesser marathons in slow times but also has a race schedule that has never lent itself to long buildups. That's changed now. He has had a true buildup to the Trials, including running a personal best of 62:28 to finish second at the Phoenix Half Marathon in January. He's won several marathons and could perhaps pick off some stop contenders late if the pace goes out too fast and he sticks with his plan. If I squint, I could imagine him getting in under 2:11.
Why Not: This is a deep cut. This is probably crazy. Bruce has never run a marathon faster than 2:20.
Why: Time and time again, Meb has proved he is a racing chameleon. Race goes out hard? Meb is waiting for you to fail. Race goes out slow? Meb is ready to close hard, from way out.
Why Not: Meb has looked mortal from time to time, but is the most experienced competitor in the field and runs smart. He'll have to break a hip, a la 2007, to be held off the podium.
Why: Rupp has proven that he is very good at letting others dictate the pace and then pouncing late in the race. He won't do any of the work and should be fast enough to keep up with whoever leads.
Why: Pennel looked outstanding in his 2014 US Marathon Championship. He's run great from every distance down to the mile (3:58) since then. I expect him to contend and possibly make this team Saturday.
Why Not: The field is strong and he'll have to have an A race, plus expect others to falter. He's held off Ritz recently, and Jared Ward; but he'll have to out duel the likes of Luke Puskedra, Matt Llano and Bobby Curtis, as well.
Why: Vail is notoriously a strong closer. If he's close with 2-3 miles to go, he'll smell blood and find his way onto the podium. Expect a 2007-esque Brian Sell type race plan from Vail.
Why Not: He's been hurt, which will affect fitness. And he'll have a strong field to contend with.
Why: Chelanga has showed brushes of greatness throughout his young career, and has proven he can run with Rupp over different distances. Expect him to lock in with Rupp and hang on as long as possible.
Why Not: It will be his debut marathon, and we all know that they don't always go swimmingly. Lots of other fast halfers like Tim Ritchie and Diego Estrada may follow his same tactic. We'll see who can hang on the longest.


His two daughters had warned him that I was probably going to ask him his age. She does not reveal it.
Only his bosses are in the secret of the gods.
Laughing heartily, Jacqueline Pelletier just reveals to me that she is the oldest employee of the restaurant where she has been working for 39 years.
The place is without presentation. Greek is always full.
Since it was founded in 1959, people from all over Quebec have made a detour on Route 138 in Trois-Rivières to stop there as a place of pilgrimage. His followers swear by his famous pizza.
Luc Corriveau knows the recipe. He has been a cook for 40 years.
He is the employee at the top of the seniority list, the living memory, the pillar, the quiet force.
He never forgot either the height of the pile of dishes to wash.
At the time, the restaurant closed in the middle of the night, but the young man never left before 5am, as long as the last utensil was not washed and wiped.
For twenty-seven and a half years, the single person was content with a single day off a week that could reach 60 hours of work.
He was a diver during the day, a cook in the evening, in addition to looking after the purchases, receiving the goods … and looking after the sheep grazing at the end of the parking lot where children come.
Some customers asked him the question before me. No, the animal named Panayotis never found himself in a recipe. Neither the first nor the others that have succeeded each other over the decades, in the small enclosure.
The sheep is not the only emblem of the restaurant Le Grec. The fustanelle too, the Greek national dress that the waitresses wear.
Jacqueline Pelletier has always been proud to wear it. This is also the case for girls who take over in 2019.
"They are anxious to have their dress!" Says the lady who is convinced that this ceremonial costume is part of the success of the restaurant.
Jacqueline owned a convenience store before offering her services at the restaurant where she dreamed of working.
The lone mother had no experience in the field, but she had this essential quality to get the job.
And the world loved her just as much.
People ask to sit in her section where the waitress goes from one table to another, in perfect control of the plates she balances on one arm, always ready to make the conversation between a coffee for sir, a tea for madame.
In this period of labor shortage, especially in restoration, Jacqueline and Luc are a rare, endangered species.
These two model employees have even grown their current bosses, Ioanna and Dimistris Yannopoulos, the third generation of homeowners.
"We've been in their legs for a long time. My brother and I were playing hide and seek around the restaurant, "says Ioanna admiringly for this duo of foolhardy loyalty and endurance.
Their respective job requires standing for hours.
While the director of Greek struggles to recruit candidates to fill the needs, Luc never felt the urge to go to another restaurant if the cauldrons were brighter.
Fortunately. Regular customers worry when they do not see him around.
"But who will prepare my favorite dish?" Have already asked the old-timers who come here up to three times a week.
Luc is never far away, probably in the second kitchen, at the back of the establishment that we had to enlarge.
Their cook is not ready for retirement that could ring in five years.
She is also that of Jacqueline who after all these years, continues to work on weekends and evenings, as in her early days.
The waitress ageless knows no better recipe than this one.


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Animal pests/
Bumper beech seed triggers pest plague
The heaviest beech forest seedfall in more than a decade is predicted this year. It is expected the increased seedfall will lead to an explosion in the numbers of rats, mice and stoats, who will turn to our native birds for food once the seeds disappear.
Beech trees generally seed every four to five years but weather conditions over the last two summers—a cool summer followed by a warm one—appear to have triggered a bumper seed or "beech mast" event. Intense and widespread flowering was witnessed throughout North and South Island beech forests during spring and early summer, prompting the need for urgent action.
Past experience has shown that when a beech mast occurs, it leads to a dramatic rise in mice and rat populations, who feast on the plentiful seed all winter. To give you an idea of how quickly they can multiply, a single female rat can potentially produce 10 offspring every eight weeks—that's a lot of rats!
An explosion in rodent numbers leads to a sharp rise in the number of stoats, which also pose a lethal threat to many species.
Rat eating fantail chicks at nest
In spring, when the seed runs out, germinates and rots, these predators will then prey on native birds and their eggs, as well as other critically endangered critters such as native bats and snails.
This will put some of our most threatened species at risk of extinction including:
– mōhua/yellowhead
– kākāriki karaka/orange-fronted parakeet
– pekapeka/short-tailed bat
– whio/blue duck
– Powelliphanta snails
Kea and tākahe are also at risk of being preyed on by stoats.
Yellowhead/mōhua
Landcare Research estimates that 25 million native birds die through predation every year in New Zealand and the beech mast is expected to make the situation much worse. For example, there are only 200–400 wild orange-fronted parakeet left and during the beech mast that occurred in 2000, 85% of the southern population was wiped out due to the rat plague.
85% of the southern population of orange-fronted parakeets were wiped out during the beech mast that occurred in 2000
DOC staff will monitor the amount of seed produced this summer and seedfall in the autumn. Rat tracking will also take place in February and May.
DOC scientist Graeme Elliott says, "So far we've only been able to get a visual idea of the issue. We've seen lots of flowering during the spring, which caused huge clouds of pollen above the forests.
"The seeds are developing at the moment but in February we'll be able to start counting them to get a better idea of the scale of the mast. We do this by shooting down branches at the top of the tree, where they're exposed to the sun and produce the most seeds.
"The best indicator will be the rat tracking. If the numbers dramatically increase or are already high in February, we'll know we've got a big problem to deal with."
Last night the Minster of Conservation, Dr Nick Smith, announced DOC's plans to respond and launched our largest-ever species protection programme called 'Battle for our Birds'. We'll talk about this in more detail over the coming weeks. For now, you can learn more about it on the DOC website: www.doc.govt.nz/battleforourbirds.
In Animal pests, Native animals, Native plants	1080, battle for our birds, beech, beech mast, Pest control, rats, stoats
4 responses to Bumper beech seed triggers pest plague
randomramblingideas 05/02/2014 at 11:14 am
Very interesting article 🙂
Jason Scott - Editor 01/02/2014 at 9:59 am
Reblogged this on Pied Piper Pest Control.
MM 31/01/2014 at 2:54 pm
There still needs to be something done to control cats feral and DOMESTIC which are now far too many and allowed to roam free day and night killing at will.
Trackbacks and Pingbacks:
The Battle for our Birds « Conservation blog	- February 11, 2014
[…] Recently we posted about the problem of increased predator numbers this year, due to predicted heavy beech forest seedfall. We also discussed what this could mean for our endangered native wildlife. […]


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Krish's VEDHAM Movie Launch Photos
Krish's multistarrer Vedam was launched at Cinemax. This film features Allu Arjun, Manoj Manchu and Anushka in the main leads. K Raghavendra Rao sounded the clapboard and K Raghavendra Rao switched on the camera. Shobu Yarlagadda and Prasad Devineni produce this movie Arka Media Works banner.
Initially planned with new faces – Krish
Krish said, "Nobody believed me when I said i am doing a multistarrer in Telugu. I was preparing script for Venkatesh's Krishnam Vande Jagadguram and there was some delay in sealing on it. I took permission from Venkatesh to do another film in the mean time. Initially i planned to make this movie with new faces. Allu Arjun has been showing interest for a while to work with me and when narrated the script, Allu Arjun came forward to do a role of slum star and it increased my levels of confidence and I could able to rope in other stars. Manoj Manchu is doing the role of a rock star. Mohan Babu also liked the story. Doing a multistarrer is not a reality in Telugu films and I would like to thank Allu Arjun and Manoj Manchu for accepting this project. There will be five important characters in this movie played by Allu Arjun, Manoj Manchu, Anushka, Manoj Bajpai and a old person. Anushka is doing a bold role. The shoot will be complete by December 2009."
Vedam is about five stories – Allu Arjun
Allu Arjun said, "People say that story is the hero for any movie. But for Vedam, director Krish is going to be the main hero. I selected a particular character after listening to the script. Manoj Manchu and Anuksha are also doing other important characters. I feel that you need two hands to clap. That is why we are putting our egos aside and doing this movie. There will be five interwoven stories in the movie and each story belongs to one of the 5 main characters. Bollywood Manoj Bajpai is doing another important character. An old man is doing the 5th character. The old character will steal the show. My uncle Chiranjeevi patted my back when i told him that i am doing a multistarrer. There is positive vibe among the team about this movie and i am confident about the success of this movie. And success of this movie will create a new trend of multistarrers."
I was supposed to act in Gamyam – Manoj Manchu
Manoj said, "I was supposed to act in Gamyam and it didn't happen. I told Krish that i wouldn't mind doing a villain role as well if he casts me. Vedam is a commercial film with international quality. I want to prove myself as an actor and I am not doing this movie for stardom. Allu Arjun met me one day and asked me if I met Krish. When I said no, he asked me to immediately meet him. I am hugely impressed by the story. I am happy to work with Bunny."


Institute of Rheological Function of Foods Co., Ltd.
Plasmalogen in phospholipid class is ubiquitously found in biological membrane. Although oxidative stress is involved in human atherosclerosis and this unique phospholipid may play a role as an endogenous antioxidant, there still remains a debate concerning the role of plasmalogen in human atherosclerosis. To investigate the relationship between plasmalogen and atherosclerosis, plasmalogen in plasma and erythrocyte membrane was quantified in atherosclerotic patients (n = 20) and age–matched control subjects (n = 20) using high–performance liquid chromatography (HPLC). In the HPLC of plasma treated with phospholipase A1, concentrations of choline plasmalogens (pl–PC) and ethanolamine plasmalogens (pl–PE) in atherosclerotic patients were significantly lower than the respective concentrations in healthy controls. In the HPLC of erythrocyte membrane phospholipid extract, the peak area of pl–PE in atherosclerotic group was reduced significantly relative to that in control group. This study demonstrated that plasmalogen in plasma and erythrocyte membrane is diminished in patients with severe atherosclerosis requiring endovascular therapy. Further studies are required to elucidate the clinical role of plasmalogen as a laboratory marker in severe atherosclerotic patients.


Boilermakers-Iron Ship Builders-Blacksmiths-Forgers & Helpers, Elizabethtown, Kentucky (January 23, 2018).
General Drivers, Warehousemen & Helpers Local Union No. 89--Louisville, Kentucky (January 29, 2018).
Kentucky State UAW Community Action Program, Louisville, Kentucky (March 15, 2018).
Kentucky State AFL-CIO's Committee on Political Education--Frankfort, Kentucky (April 16, 2018).
Tri-County Council of Labor--Henderson, Kentucky (June 21, 2018).
International Brotherhood of Electric Workers Local 1701--Owensboro, Kentucky (June 26, 2018).
Kentucky State Building and Construction Trades Council--Louisville, Kentucky (Aug. 12 2018).
Jefferson County Teachers Assoc.—Louisville, Kentucky (September 13, 2018).
International Union of Painters and Allied Trades District 91 (October 16, 2018).
22 Strong Veterans Group—Paintsville, Kentucky (October 17, 2018).
Joan Hoffman, Mayor City of Henderson 1999-2002 (February 4, 2018).
Dr. David Watkins, State Representative 2007-2016 (February 5, 2018).


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India is still plagued with Dowry System, a system that has been a curse to many struggling families. Parents cut down on their food to save enough money to pay for the dowry of their daughter. Daughters have remained unmarried if parents could not afford the dowry; daughters have been tortured, physically and mentally; daughters have been divorced, kicked out, and killed, if the dowry was less; daughters have been aborted before they were born because of fear of dowry. This heinous tradition has to stop. Meri Bahu is strictly against the dowry system and requests its members not to follow the traditional path of dowry. At our discretion, we reserve the right to cancel the membership of a user if a complain of dowry is received.


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Brownback Proclaims January as Human Trafficking Awareness Month
KANSAS CITY, KAN. ---- Kansas Governor Sam Brownback, along with Attorney General Derek Schmidt, Secretary Phyllis Gilmore, Kansas Department for Children and Families (DCF), Secretary Lana Gordon, Kansas Department of Labor (KDOL), Secretary Ray Roberts, Kansas Department of Corrections (KDOC) and Interim Secretary Susan Mosier, Kansas Department of Health and Environment (KDHE) have proclaimed January as Human Trafficking Awareness Month in Kansas.
"I take seriously the fight against human trafficking," Governor Sam Brownback said. "We have trained more than 500 child welfare professionals about human trafficking rings making Kansas a national model for preventing this horrendous crime."
Human trafficking is a form of modern-day slavery in which victims are lured, forced, or coerced for the purpose of commercial sex, debt bondage or forced labor. Kansas' location and interstate system make it a major transportation area for victims of human trafficking.
"It's up to each person in the community to identify and report suspected commercial sexual exploitation of a child," DCF Secretary Phyllis Gilmore said. "These children do not choose to be exploited; they are children who deserve our protection."
The number of human trafficking victims served by victim service agencies through the state that received grants from the Attorney General's office was 338 in fiscal year 2014; this is up from 218 in 2013.
"Kansas has adopted new laws that seek to protect and rescue human trafficking victims – especially children," Kansas Attorney General Derek Schmidt said. "Kansas now has increased penalties and put in place other measures to enhance the prosecution of traffickers and buyers in a comprehensive effort to reduce sexual exploitation and other trafficking statewide."
The bill defines commercial exploitation of children, which does not require a showing of force, fraud, threat or coercion and references the existing statutory definition of human trafficking and aggravated human trafficking.
"House Bill 2034 strengthened our ability to prosecute labor traffickers, but it is still a big problem," KDOL Secretary Lana Gordon said. "While we have made immense strides with the bill, we cannot stop there and need to continue fighting. If you or someone you know is working under unfair conditions, report it."
Labor trafficking is the recruitment, harboring, transportation, provision or obtaining of a person for labor or services, through the use of force, fraud or coercion.
"The Kansas Department of Health and Environment works to protect the health and ensure the safety of all Kansans. Victims of human trafficking are especially vulnerable," said Acting Secretary Susan Mosier, M.D. "We work to protect these victims by educating schools and other partners on the signs of human trafficking in addition to regulating the facilities in which they are placed."
The Governor along with the Attorney General's office, DCF, KDHE, KDOC and KDOL are working together to educate Kansans about the presence of human trafficking, what to look for and how to report suspected human trafficking. Educational information is provided on the agencies' websites.
"The Kansas Department of Corrections is pleased to be an active participant in the human trafficking task force," KDOC Deputy Secretary Terri Williams said. "The task force has given us the opportunity to work with juveniles, many of whom are both offenders and victims, through a cooperative, unified interagency forum that involves trauma-informed care."
For more information on Human Trafficking go to https://ag.ks.gov/childrens-safety/human-trafficking.
Labels: Human Trafficking Awareness Month, Politics, Sam Brownback


Broadly is a website and digital video channel devoted to representing the multiplicity of women's experiences. Through original reporting and documentary film, we provide a sustained focus on the issues that matter most to women. As one SV-film commenter succinctly put it: "So basicly [sic] vice but excluding anything of relevance that includes men."


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Q: Append multiple records from each loop iteration in PL/SQL I am trying to write a procedure in Oracle PL/SQL that looks like below snippet:
    > LOOP:
         >READ INPUT FROM CURSOR
         >GET OUTPUTS USING SELECT QUERY(OUTPUT RECORD COUNT MAY VARY ON EACH ITERATION)
         >APPEND OUTPUT TO SOME DATA STRUCTURE
    > END LOOP;
    >RETURN DATA STRUCTURE

Actually I am stuck with this appending task. In each iteration different number of output will be available using a select query. I want to append all of the records in a single data structure.
Suppose inner select query return 3 columns ColA,ColB,ColC and the loop iterates 2 times. Then in 1st iteration it returns:
1,2,3
3,4,5
In the next iteration it returns 4,5,7.
The procedure will return some data structure containing below:
1,2,3
3,4,5
4,5,7
Is there any way?

A: I guess this can be solved with pipelined  functions.
So it will look something like this:
declare a type
 TYPE my_record is RECORD(
       cola      number,
       colb      number,
       colc       number);

TYPE my_table IS TABLE OF my_record;

a function
function  get_results()  RETURN my_table PIPELINED is
    my_rec   my_record:=null;
    cursor myCursor(data number) is
    --some select expression
    ;

    begin

    --loop through outputs

     FOR item IN myCursor(data)  LOOP
      my_rec:=null;
      select item.value1,item.value2,item.value2 into rec from dual;
      PIPE ROW(my_rec);
     end loop;
    return;

    end;

and finally use it
SELECT * FROM TABLE(get_results);

redpajama_set_name: RedPajamaStackExchange


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John Gibb Bothwell (1909 or 1910 – 1994) was a British trade union leader.

Bothwell became a junior clerk with the London and North Eastern Railway when he was sixteen years old.  He joined the Railway Clerks' Association, and from 1939 began working full-time in its Scottish office.  In 1950, he was appointed as the Scottish secretary of the union.  He became active in the Scottish Trades Union Congress, and served as its president in 1954.  In 1956, he was made an Officer of the Order of the British Empire.

In 1960, Bothwell was elected as assistant general secretary of the union, by now renamed as the Transport Salaried Staffs' Association (TSSA).  He became general secretary in 1963, and was also elected to the General Council of the Trades Union Congress, and in 1965 to the general council of the International Transport Workers' Federation.  He retired from his trade union posts in 1968, due to poor health.  However, he remained active as a member of the Industrial Arbitration Board, for which work he was made a Commander of the Order of the British Empire.

References

General Secretaries of the Transport Salaried Staffs' Association
Members of the General Council of the Trades Union Congress
20th-century births
1994 deaths
Year of birth uncertain


Apple Inc. (NASDAQ:AAPL) is preparing for CEO Tim Cook's keynote speech at its annual Worldwide Developers' Conference (WWDC). The speech is scheduled for today at 10 a.m. Pacific (1 p.m. Eastern) at the Moscone Center in San Francisco.
Apple Insider has taken a peak at the outside of the building and notes that in addition to the typical iOS 8 and WWDC14 banners, there are also several others that are covered up. It's pretty typical for Apple Inc. (NASDAQ:AAPL) to do this sort of thing. According to the website, the iOS 8 and WWDC14 banners are on the ground floor of the Moscone Center, where registration is already taking place. Apple is keeping anyone from going upstairs, however.
Those on site can see some banners that are covered up two levels higher. Apparently it's possible to see the tops of some banners that are partially covered on the floors that are higher up. However, there's still no telling what's on the banners.
What may lurk behind Apple's hidden banners?
Apple Inc. (NASDAQ:AAPL) CEO Tim Cook could tell us more about what's on those banners in today's keynote speech. There are a couple of interesting notes on Apple's schedule for tomorrow at WWDC. At 9 a.m. Pacific on Tuesday, Apple has something listed as "No Comment" under Tools and another item listed as "This One Is Sealed" under Media. There's also a third one titled "Shhhh, Can't Tell You Yet" under Graphics and Games and a fourth one titled "It's Under Wraps" under Core OS at the same time.
We've heard plenty of rumors leading up to WWDC already. Of course there are the usual things, like the unveiling of iOS 8 and all of its updates. Apple Inc. (NASDAQ:AAPL) is also expected to show off the next version of its Mac OS X 10.10. Some have said we'll also see a new health monitoring app called Healthbook. Other possibilities include more details on the Beats Electronics acquisition and Apple's plans for home automation.
If you aren't personally attending Apple Inc. (NASDAQ:AAPL)'s WWDC this year, you can also catch today's keynote speech via the live stream right here. In order for it to work though, you must have Safari 4 or later running on OS X 10.6 or later or Safari on iOS 4.2 or later. Those who want to watch it on their Apple TV must have a second- or third-generation box running software 5.0.2 or later.