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

Cataclysmic variables (CVs) are close binary systems comprised of a white dwarf (WD) and a low-mass star losing matter in a  Roche-lobe
overflow regime, usually creating an accretion disc around the accreting WD \citep{1995CAS....28.....W}. CVs show diverse observational
characteristics depending on fundamental physical properties, including their orbital period,  mass transfer rate; and strength of the
magnetic field of the WD. Their diversity is also in part due to the viewing angle \citep{2018AJ....156..198H}.  In non- or weakly-magnetic
systems, the accretion flow takes place in a fully-developed accretion disc.  At high mass transfer rates ($\ge 10^{-9}$~M$_{\sun}$\,yr$^{-1}$),
these are hot, steady-state discs  \citep{1996MNRAS.282...99B}. Therefore,  the disc thermal instability that triggers dwarf nova outbursts
is prevented \citep{1986ApJ...305..261S,1992ApJ...394..268S,2001NewAR..45..449L}. These high mass transfer rate systems are known as
nova-like variables (NLs), because it was initially argued that they might potentially exhibit or have undergone undetected nova eruptions
\citep{1934Obs....57..157V}. No known NL has ever been seen to erupt as a nova.  However, some NLs may resemble  nova when the nova returns to a quiescent state after the eruption \citep{1995CAS....28.....W}. They constitute a small fraction of the entire CV
population \citep[$\sim$15\ percent  in][]{2003yCat.5113....0R, 2003A&A...404..301R},
which might be result of an observational bias. The vast majority of NLs have orbital periods  above the so-called "period gap"
\citep{1983ApJ...275..713R,1998MNRAS.298L..29K,2016MNRAS.457.3867Z,2020MNRAS.492L..40A}. We exclude  CVs with moderately or highly magnetic WDs, which historically were also accounted for as NLs.

There is a visible differentiation between NLs and  dwarf novae in terms of their orbital periods and colours \citep{2020MNRAS.492L..40A}.
It is noticeable that NLs dominate the orbital period range 3-4h, where very few dwarf novae are observed \citep{2011ApJS..194...28K}.
However, in absolute numbers, the amount and the distribution of NLs and dwarf novae right above the period gap are comparable
\citep{2011ApJS..194...28K}. There is no good understanding why the two populations of NL and dwarf novae overlap in some period ranges,
but not in others. NLs have accretion rates that are higher than "normal" CVs both at longer and shorter periods. They are intrinsically
very bright, and their WDs  tend to be hotter \citep{2009ApJ...693.1007T}.

\begin{table}
  \setlength{\tabcolsep}{0.1em}

    \caption{Log of  spectroscopic observations}
    \label{tab:speclog}
    \begin{tabular}{lccccc}
       \hline \hline

Date   & JD$^*$ & Range~~~   & No. of   & ~~~Exp. time & ~~~Comments \\
      &         & (\AA)~~~~~ & Spectra  & (s)          &             \\ \hline
2002 Aug. 21 & 2507     &    3341-7546    &            2  & 200  &  INT       \\
2002 Aug. 23 & 2510    &    3341-7546    &            24 & 340  &  INT       \\
2002 Aug. 25 & 2512    &    3341-7546    &  15 & 120  &  INT       \\
2002 Aug. 31 & 2518    &    3341-7546    &            8 & 120  &  INT       \\
2002 Sep. 02 & 2520    &    3341-7546    &            4 & 120  &  INT       \\
2002 Sep. 03 & 2521    &    3341-7546    &            6 & 120  &  INT       \\
2003 Oct 19  & 2932         &  3784-9063      &             2  &   60   & ISIS B\&R  \\
2003 Dec. 13   & 2987    &    4257-8318    &             4 &   120   &  CA         \\
2003 Dec. 14   & 2988    &    4257-8318    &             9 &   60   &  CA         \\
2003 Dec. 15   & 2989    &    4257-8318    &             2 &   60   &  CA         \\
2003 Dec. 16   & 2990    &    4257-8318    &             10 &   60   &  CA         \\
2003 Dec. 17   & 2991    &    4257-8318    &             10 &   60, 120   &  CA         \\
2003 Dec. 17   & 2991    &    3775-6840    &             7 &   120   &  NOT         \\
2003 Dec. 23   & 2997    &    4257-8318    &             6 &   60   &  CA         \\
2003 Dec. 24   & 2998    &    4257-8318    &             6 &   60   &  CA         \\
2003 Dec. 25   & 2999    &    4257-8318    &             2 &   60   &  CA         \\
2003 Dec. 26   & 3000    &    4257-8318    &             4 &   60   &  CA         \\
2003 Dec. 27   & 3001    &    4257-8318    &             2 &   60   &  CA         \\
2004 Aug. 09   & 3226    &    4257-8318    &             2 &  180    &  CA         \\
2004 Aug. 10  & 3227    &    4257-8318    &             2 &  180   &  CA         \\
2004 Aug. 11  & 3228    &    4257-8318    &             2 &  180    &  CA         \\
2004 Aug. 12  & 3229    &    4257-8318    &             2 &  180    &  CA         \\
2004 Oct. 21  & 3300    &    4257-8318    &             2 &  120    &  CA         \\
2004 Oct. 23  & 3302    &    4257-8318    &             2 &  120    &  CA         \\
2004 Oct. 24  & 3303    &    4257-8318    &             2 &  120    &  CA         \\
2004 Oct. 26  & 3305    &    4257-8318    &             2 &  120    &  CA         \\
2004 Sep. 10  & 3623    &    4257-8318    &             2 &  120    &  CA         \\
2004 Nov. 04  & 3314    &   3775-6840     &                  2 &  120    &  NOT      \\
2005 Jan. 01   & 3372    &    3784-9063    &             2  &  200    & ISIS B\&R  \\
2005 Jan. 04   & 3375    &    3784-9063    &             2  &  200    & ISIS B\&R  \\
2005 Jan. 05   & 3376    &    3784-9063    &             2  &  200    & ISIS B\&R  \\
2005 Jan. 06   & 3377    &    3784-9063    &             2  &  200    & ISIS B\&R  \\
2005 Jan. 07   & 3378    &    3784-9063    &             2  &  200    & ISIS B\&R  \\
2005 Sep. 10  & 3623         &    4257-8318    &             2 &   120   &  CA         \\
\hline
2017 Oct. 27     & ~~~~~8053~~~~~    & 3600--7300 & 3 & 1200 & Echelle \\
2017 Oct. 28     & 8054     & 3600--7300 & 3 & 1200 & Echelle \\
2017 Oct. 29     & 8055     & 3600--7300 & 3 & 1200 & Echelle \\
2018 Jan. 11     & 8129     & 3600--7300 & 13 & 1200 & Echelle \\
2018 Jan. 12     & 8130     & 3600--7300 & 12 & 1200 & Echelle \\
2018 Jan. 13     & 8131     & 3600--7300 & 3 & 1200 & Echelle \\
2018 Jan. 14     & 8132     & 3600--7300 & 10 & 1200 & Echelle  \\ \hline

 \end{tabular}

\begin{tabular}{l}
$^*$ 2450000+
JD is given at beginning of the observing night.
\end{tabular}
\end{table}

The spectra of some NL variables display persistent broad Balmer
absorption lines, indicative of optically thick discs. However, NLs themselves come in different flavours.
A fraction of NLs, known as  VY\,Scl stars, show  occasional states of low mass transfer rates, i.e. they become significantly
fainter for prolonged periods of time \citep[months to years,][]{1974Obs....94..116W,2020MNRAS.494..425R}.
However, the physical cause of these low mass transfer states is still uncertain \citep{1994ApJ...427..956L,1998ApJ...499..348K,2018A&A...617A..16S}.

SW\,Sex stars form a class of NL variables with distinctive spectroscopic behaviour \citep{1991AJ....102..272T}.
They mostly cluster in the 3-4\,h orbital period range \citep{10.1111/j.1365-2966.2007.11743.x}.
\citet{1996MNRAS.282...99B}, \citet{2013MNRAS.428.3559D}, and \citet{2014AJ....147...68T} proposed an extended hot
spot as the predominant source of emission lines  from the optically and physically thick disc. However, such interpretation
is challenged by \citet{2007MNRAS.377.1747R,2015MNRAS.452..146R}.
A search for non-eclipsing SW\,Sex in the 3-4\,h period range revealed systems with
two-component emission lines \citep{10.1111/j.1365-2966.2006.11245.x}, but they were inconclusive whether these are low-inclination
SW\,Sex objects.
Conversely,  two-component emission lines recently have been observed,  in a couple of  the UX\,UMa-type NLs (which are
the primary concern of this paper).
For example, \citet{2017MNRAS.470.1960H}, based on high-resolution spectroscopy,  demonstrated  that NLs RW\,Sex and
RXS\,J064434.5+334451  show at least two components in the profiles of  the Balmer emission lines.
The narrow component with a low radial-velocity amplitude originates
from the irradiated surface of the secondary facing the disc.
The wide component
is formed in an extended, low-velocity region in the outskirts of the opposite side of the accretion disc, with respect
to the collision point of the accretion stream and the disc. Recently, \citet{Subebekova20} claim, that this property is
observed in RW~Tri.  They  compiled  a current list of similar NLs  with orbital periods
$\geq$4 hours. At least four of them, the components of H$\alpha$ emission
 closely resemble those seen in RW\,Sex.

Other interpretations of line provenance (including absorption features frequently flanking emission lines) in such NL systems have
been put forward. Notably, the disc overflow model  by \citet{1996ApJ...471..949H} and disc wind interpretations and models
\citep[e.g.][]{1996AJ....111.2422P,1996Natur.382..789M} are worth mentioning.

BG\,Tri\ is a bright object reported by \citet{2004AJ....127.2436W,2008PZP.....8....4K} to show an irregular, low-amplitude variability and
tentatively identified as a CV, citing ROTSE1, TYC2 and {\it ROSAT} detections. Accordingly, the object is also catalogued as
TYC\,2298\,01538 and 1RXS J014448.4+323320. \citet{2017RMxAA..53..439M}  confirms its NL identification based on a distance estimate
by {\it Gaia}\footnote{ $d= 334.013 \pm 7.65 $\,pc according to the revised estimate \citet{Bailer18}} \citep{2018AA...616A...1G} in combination with Galaxy Evolution Explorer {\it (GALEX) UV} magnitudes \citep{2003SPIE.4854..336M}. However, BG\,Tri\ has not been
studied in detail until now. We report the results of the spectroscopic study of the object on the backdrop of the long term
photometry collected by the Catalina Real-time Transient Survey and the All Sky Automated Surveys (ASAS).

\section{Observations and Reduction}
\label{sec:observations}
We  present an extensive set of multi-wavelength observations of BG\,Tri\  obtained  by us as well as a variety of data collected in surveys.

\subsection{Photometry}

\begin{figure}
\setlength{\unitlength}{1mm}
\resizebox{15.cm}{!}{
\begin{picture}(130,72)(0,0)
\put(-5,0) {\includegraphics[width=8.0cm, bb=0 180 580 700, angle=0, clip]{Fig1-bg.eps}}
\end{picture}}
\caption{
 Long-term light curve of BG\,Tri\ obtained by the sky  patrol ASAS SN and CRTS surveys. The dark green and orange points are ASAS
 data in $V$ and $g$ filters respectively, the light green  points are CRTS $V$-band data. In the lower panel, the entire data set is
 presented, while the upper shows expanded segment of the same during and around the low state. The magenta markers indicate moments of
 spectroscopic observations at the bottom of the light curve. }
\label{fig:lccurve}
\end{figure}

\begin{figure*}
\setlength{\unitlength}{1mm}
\resizebox{15.cm}{!}{
\begin{picture}(130,80)(0,0)
\put(-15,0) {\includegraphics[width=15.75cm, bb=0 160 580 520, angle=0, clip]{Fig2-bg.eps}}
\end{picture}}
\caption{
 The combined and averaged low-resolution spectrum of BG\,Tri\  obtained at different epochs with different instruments.
 Major lines identified in the spectrum are marked on top, while atmospheric oxygen lines are marked at the bottom.  \ion{Mg}{i} triplet is
 also marked, although we are not sure if it is real.}
\label{fig:lowres}
\end{figure*}

\begin{figure*}
\setlength{\unitlength}{1mm}
\resizebox{15.cm}{!}{
\begin{picture}(130,75)(0,0)
\put(-15,0) {\includegraphics[width=8cm, bb=0 140 570 700, angle=0, clip]{Fig3a-bg.eps}}
\put(60,0) {\includegraphics[width=8cm, bb=10 140 580 700, angle=0, clip]{Fig3b-bg.eps}}
\end{picture}}
\caption{
 The profiles of important lines in the spectrum of BG\,Tri\ from the echelle spectra. The lines are marked in upper corners of each panels. The
 black line is the median of all high-resolution spectra,  whether the low resolution spectrum from Figure\,\ref{fig:lowres} are presented
 in the background.}
\label{fig:lines}
\end{figure*}

The data from the Catalina Real-Time Transient Survey (CRTS) \citep{2009ApJ...696..870D} and the All-Sky Automated Survey for Supernovae
(ASAS SN) \citep{2014ApJ...788...48S,2017PASP..129j4502K}  were used to produce the light curve  (Figure\,\ref{fig:lccurve}) of the object.
The data were obtained in $V$- and $g$-bands. The difference between filters $g$ and $V$ is not significant and the average colour index
was $g-V\approx0.0$.
Most of the time  BG\,Tri\ is bright ($\approx$12~mag, one of the brightest CVs in apparent magnitude) and nearly constant with  non-regular, small amplitude variability. The average magnitude in a time stretch HJD 2456524.01 to HJD 2457668.08 is $V=11.91$, with a deviation
of $\approx$0.06 magnitudes.  The light curve shows one occasion
of a large flux drop ($\sim2.5$\,mag), with a duration of 176\,days.
The initial descent from the average $V\approx11.9$ to $\approx$13.6
magnitude lasts about 40\,days at a rate of 0.04\,mag~day$^{-1}$.
Following a stand-still at that magnitude that last one month,  the brightness briefly falls further (on HJD\,$2458373$), reaching
$V=14.3$\,mag. From there, the luminosity starts to recover with a slower rate of 0.026\,mag\,day$^{-1}$.
This low state episode,  detailed in the upper panel of Figure\,\ref{fig:lccurve}, is fairly common among NLs,
classifying BG\,Tri as a VY\,Scl star.
There is also an episode of a sudden jump of brightness detected between HJD\,2457669.88 and HJD 2457797.72 before
the anti-dwarf nova episode when the average brightness of the object reaches $V\approx11.7$.

\subsection{Spectroscopy}

\subsubsection{Low-resolution spectroscopy}

A large number of low-resolution spectra were obtained with a variety of instruments listed in Table\,\ref{tab:speclog}.
At the 2.5-m Isaac Newton Telescope (INT), we used the Intermediate Dispersion Spectrograph (IDS) with the R632V grating,
the $2048\times 4100$ pixels EEV10a CCD detector, and a 1\farcs1 slit width. With this setup, we sampled the wavelength region 4400 - 6700~\AA\
at a  full width at half maximum FWHM of $\sim$2.5~\AA\ resolution.
More spectra were obtained using the blue arm of the Intermediate dispersion Spectrograph and Imaging System (ISIS) mounted on the 4.2\,m
William Herschel Telescope, at the Roque de los Muchachos Observatory on La Palma. Spectra of Cu-Ne-Ar comparison lamps were obtained every
$\sim$30--40\,min in order to secure an accurate wavelength calibration.

Additional data was obtained with the Andaluc\'ia Faint Object Spectrograph and Camera (ALFOSC), at 2.56m Nordic Optical Telescope (NOT) on La Palma. The $\#$8 CCD which has $2048\times2048$ pixel EEV chip was used for this observations. A spectral resolution of  FHWM $\sim 3.7$~\AA\  was achieved by using the grism $\#$7 (plus the second-order blocking filter WG345) and a 1" slit width. The useful wavelength interval this configuration provides is $\lambda$\,3800-6800~\AA.  The spectroscopy at the 2.2m Calar Alto  (CA) telescope was performed with CAFOS. A 1\farcs2 slit width and the G-100 grism granted access to the $\lambda$\,4200-8300~\AA\ range with a resolution of FWHM$\sim 4.5$~\AA\  on the standard SITe CCD ($2048\times2048$ pixels).
After the effects of bias and flat field structure were removed from the raw images, the sky background was subtracted. The one-dimensional
target spectra were then obtained using the optimal extraction algorithm of \citet{Horne86}. For wavelength calibration, a low-order
polynomial was fitted to the arc data, the rms was always smaller than one tenth of the dispersion in all cases. The pixel-wavelength
correspondence for each target spectrum was obtained by interpolating between the two nearest arc spectra. The preliminary reduction steps  for all low-resolution spectra were performed with the standard packages for long-slit spectra within {\sc 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.}, while wavelength calibration and most of the subsequent analyses made use of Tom Marsh's {\sc molly}\footnote{{\sc molly} is
available at Tom Marsh' web page: http://deneb.astro.warwick.ac.uk/phsaap/software/} package.

No flux calibration is available for the low-resolution spectra, hence we present in Figure\,\ref{fig:lowres} normalized spectrum
obtained by combining data at different epochs with different telescopes/instruments. The low-resolution  spectra failed to reveal
significant radial velocity (RV)  variation.

The overall spectral behaviour of
BG\,Tri\ does not change significantly from epoch to epoch. The spectra indicate a steep blue continuum with Balmer lines showing emission features embedded in broader absorption lines.
The higher members of the Balmer series appear to have  more intense absorption, while towards the lowest numbers the emission component
dominates. Helium lines are also present in the spectrum. The neutral helium lines
have complex profiles, especially at \ion{He}{I} $\lambda4471$\,\AA. Also visible are \ion{He}{ii} and \ion{Ca}{ii} lines.
The spectra are typical of NL variables  with an optically thick disc and low inclination.

\subsubsection{High-resolution spectroscopy}

The high-resolution observations were obtained with the echelle REOSC
spectrograph \citep{Levine1995}, attached to the 2.1m Telescope of the Observatorio Astron\'omico Nacional
at San Pedro M\'artir, during several nights of 2017 and  2018. The
CCD $2048\,\times\,2048$ detector was used to obtain a spectral resolution of R${\sim}18\,000$. All  observations were carried out with the
300~{l}~mm$^{-1}$ cross--dispersor, which has a blaze angle at around 5500~\AA. The spectral coverage was about $3600$--$7300 $ \AA. The
exposure time for each spectrum was 1200~s.  Th-Ar lamp was used for wavelength calibration. The spectra were reduced using the {\it
echelle} package in {\sc iraf}.   Standard procedures, including bias subtraction, cosmic-ray removal, and wavelength  calibration, were
carried out.
No flat-field correction and flux calibration was attempted; instead, the normalised spectra were used for measurements and visualisation.  The log of all
spectroscopic observations is shown in Table~\ref{tab:speclog}.

\begin{figure}
\includegraphics[angle=0,trim=0 0 0 0,width=9cm]{Fig4-bg.eps}
\caption{
 The power spectra  of  BG\,Tri\ calculated for the  radial velocity curves of different lines and components.  In the upper panel the red and
 blue lines are the power of the HVC and the LVC after the  decomposition of  H$\alpha$ line. In the inset a zoom on the small range of
 frequencies around the derived period are presented. The bottom panel shows the power of H$\beta$  measured with a single Gaussian. }
\label{fig:power}
\end{figure}

\begin{figure*}
\setlength{\unitlength}{1mm}
\resizebox{15.cm}{!}{
\begin{picture}(130,60)(0,0)
\put(-10,0) {\includegraphics[width=15cm, bb=50 500 580 720, clip=]{Fig5-bg.eps}}
\end{picture}}
\caption{
 RV curves of H$\beta$ and components of H$\alpha$ folded with the orbital period are in the left and right panels respectively. RV of
 H$_\beta$ line was first measured by fitting a single Gaussian, which enabled determination of the orbital period.  H$_\alpha$ was separated
 into two components; by fitting two Gaussians (see the text for the description). The RV measurements corresponding to the high-velocity
 component of H$\alpha$ are marked by red symbols and the fit to them  with 121\,km~s$^{-1}$ semi-amplitude as a red line. Respectively,
 the low-velocity component is plotted in blue. The semi-amplitude of the best fit curve is 74\,km~s$^{-1}$.  }
\label{fig:rvcurves}
\end{figure*}

\begin{figure}
\includegraphics[width=8.75cm,bb=20 150 580 700, clip=]{Fig6-bg.eps}
\caption{
 The line profile phase-evolution of H$\alpha$. Four orbital phases (marked in the upper right corner of each panel) are displayed. In the
 upper panels the grey line are the observed spectra. Two Gaussians obtained as a result of de-blending are plotted by red and blue curves.
 Their sum is plotted by a black line as a fit to the observed profile. In the bottom panels by the red and blue lines the residuals of
 subtraction of the counterpart Gaussian are plotted, while the gray line is after subtraction of both Gaussians.}
\label{fig:profiles}
\end{figure}

\section{The phenomenology of BG\,Tri.}
\label{subsec:sed}

\citet{2008PZP.....8....4K} in a discovery note, points out that BG\,Tri\ is a variable star, probably a CV. Presented here, the long term light curve and spectra leave no doubt that the first assessment was correct. However, CVs comprised of a WD and a late red or brown dwarf secondary star come in different flavours depending on their orbital periods (or separation), mass accretion rate,  and strength of the magnetic field of
the WD. Absence of nova or dwarf nova outbursts in a period of time over 5000\,days indicates that this is an NL variable. Moreover, an
anti-dwarf nova occurrence registered in the light curve is another characteristic of bright NLs, which occasionally undergo a fall in
brightness by more than one magnitude \citep{1995CAS....28.....W}.

Low-resolution spectra confirm the CV identification of BG\,Tri, which exhibits a standard set of hydrogen and helium lines, with higher numbers
of the Balmer series showing wide adsorptions with embedded, relatively narrow emissions. In Figure\,\ref{fig:lowres}, an averaged and
combined spectrum obtained at different epochs is plotted. All significant spectral features are marked.
A combination of emission and absorption features of Balmer lines  usually occurs  either in dwarf novae near period minimum  where the WD becomes dominant, or, in NLs with optically thick discs.

Using the {\it Gaia} distance d= 334(8)\,pc to BG\,Tri,   we calculate the absolute magnitude of the object M$_V=4.26$.
Such high luminosity enlists BG\,Tri\ among the brightest CVs, making it only the second after the infamous RW\,Sex \citep{2020MNRAS.496.2542H}.
The derived absolute magnitude is consistent with the  low inclination angle \citep{1986MNRAS.222...11W,1987MNRAS.227...23W}.  We will detail spectral energy distribution (SED) and luminosity of the accretion disc further in the paper. Nevertheless, based  only on the derived absolute magnitude, we can state that this object is not a low accretion rate WZ\,Sge type,  near the period minimum.

In NLs, the bulk of the accretion disc is optically thick (hot and dense), producing absorption lines.  The emission lines are formed either in the separate parts of the disc or by the gas in its vicinity \citep{warner_1976,1992A&A...256..433B}. Figure\,\ref{fig:lines} displays a set
of \ion{H}{i} and \ion{He}{i} line profiles from averaged, and normalised high-resolution echelle spectra (with low-resolution profiles in
the background), illustrating the composition of lines. In the averaged spectra, the emission profile of the Balmer lines  is   rather symmetric.
The absorption  is much wider,  visually slightly blue-shifted in regard to the emission peak. Measuring this shift in spectra not corrected for the instrumental sensitivity is complicated since the continuum is not well defined.

H$\alpha$ looks like it has a P\,Cyg profile with a blue-shifted absorption  from a material rapidly expanding in the direction of the
observer. However, it is just a contrast effect, particularly in the case of the low-resolution spectra. The emission feature is the
strongest among the Balmer lines, hence the symmetry of the underlying absorption line is visually distorted. However, the composition of the
line is similar to the rest of the Balmer lines; an emission peak is embedded in a wider absorption line.
Helium lines show a more complicated structure comparison with Balmer lines, discussed below.

In general, BG\,Tri's spectrum looks like a replica of RW\,Sex \citep{2017MNRAS.470.1960H} or IPHASX\,J210204.7+471015 \citep{2018ApJ...857...80G}. Hence, our approach to interpreting  BG\,Tri\  builds on the assumption that it is a low inclination NL system.

\begin{figure*}
\setlength{\unitlength}{1mm}
\resizebox{15.cm}{!}{
\begin{picture}(130,100)(0,0)
\put(-10,0) {\includegraphics[width=13.5cm, bb=0 460 390 760, clip=]{Fig7-bg.eps}}
\end{picture}}
\caption{The trailed observed and reconstructed  spectra of H$\alpha$ components along with the Doppler maps are presented here.
In the left side  the separated HVC trailed spectrum and its reconstruction are plotted at the bottom, while the corresponding velocity
map of the HVC is displayed above. Respectively, on the upper right side of the figure is the Doppler tomogram of the LVC with the
separated observed and reconstructed trailed spectra at the bottom.
The Keplerian velocity of the disc in the Doppler maps is located at  $ \upsilon_{\mathrm {disc}}\sin (i) \ge 220$\,km\,s$^{-1}$ and
the circle shows the disc external radius. The system parameters discussed in the text.
}
\label{fig:tomo}
\end{figure*}

\section{Radial velocities and period determination }
\label{sec:period}

Low-resolution spectra did not provide information on the orbital motion of emission lines.  This supports our assumption of a low orbital
inclination. Hence, we obtained higher resolution echelle spectra to reveal the orbital period of the object.
Fitting H$\alpha$  emission with a single Gaussian produced a large scatter but no definite periodic pattern.
However, measuring H$\beta$ with a single Gaussian produced a time series which allowed us to determine a possible period and its closest
one-day alias. The power spectrum calculated using a discrete Fourier transformation provided by  Period\,04
\citep{2014ascl.soft07009L,2005CoAst.146...53L} indicated that the orbital frequency was either $\sim$5.3~cycles-per-day (c/d) or
$\sim$6.3~c/d (see the bottom panel of Figure\,\ref{fig:power}). It was clear that the complications related to the period determination
were due to lines that are composed of two or more components, as evident from the study of similar objects
\citep{2017MNRAS.470.1960H,2018ApJ...857...80G}.

Now that we have an estimate of the orbital period, we
further improve the obtained result by measuring individual components of the lines.
In the high-resolution spectra, the H$\alpha$ line is the strongest feature. It is also the least affected by the absorption accompanying all H
emission lines. In general, it looks like a one peak line, but with variable wings. We applied line de-blending {\sl splot}-procedure in
{\sc iraf} to separate the line into  components.
We fit the profile with two Gaussians with unrestricted parameters.
The details of the  method are provided in \citet{2018ApJ...869...22T}.

We seek a periodic sinusoidal pattern in the RV/time-space by eye, and assign measurements of RVs to one or more
component(s), in all cases when they are clearly distinct.
Sometimes just one component stands out.
We determine a more accurate orbital period by subjecting the first emerging periodic pattern to the Fourier analysis. Period\,04 was
used to determine the best choice of the orbital period. We refine RVs by fitting a $sin$-curve to the measurements of the better-defined
component and perform another round of de-blending, by fixing the central wavelength of this component. As a result, we improve the
determination of the second component, which can be used to measure the orbital period. The difference in values of the orbital period
from two components is rather small.   The higher velocity amplitude component (HVC) power spectrum peaks at 6.31114\,c/d, while the lower
velocity amplitude  component (LVC) has a frequency of 6.33794\,c/d. The spread of measurements remains high. The residuals (RMS) of the fit of
HVC are 36\,km~s$^{-1}$ with the amplitude of variation 121\,km~s$^{-1}$. The LVC has an amplitude of 78\,km~s$^{-1}$ and
RMS of 25\,km~s$^{-1}$.  They reconcile better at the period determined from the HVC, which we adopted as the orbital period of
P$_{\mathrm {orb}}=3.8028(24)$\,h = 0.15845(10)\,d.
The power spectra obtained from RVs of H$\beta$ and two components of H$\alpha$ are presented in Figure\,\ref{fig:power}. Obviously, the power
of H$\beta$ as a whole is much smaller than the power of separate components of H$\alpha$, but they all are consistent with one another.

The RV curves of H$\beta$  and H$\alpha$ components along the measurements folded with the determined orbital period are presented in the two
middle panels of Figure\,\ref{fig:rvcurves}, respectively. We assigned phase zero at the negative to positive crossing of the LVC.  Plots are
flanked by trailed spectra of corresponding lines on both sides.
In the upper panel of Figure\,\ref{fig:profiles} Gaussian profiles of individual components, their sum, and the observed line profiles in four
different orbital phases are presented to illustrate the result of the separation of the line  into two components. Residual spectra of individual components,  as well as residuals after subtraction of both components, are displayed in the bottom panel.
H$\beta$ is probably also multi-component, but dismantling  it into components is rather difficult. There is a stronger absorption
undermining the wings of the emission components. One component (the HVC) dominates, as evident from Figure\,\ref{fig:rvcurves}. The amplitude of fitted $sin$-curve to single-Gaussian measurements of the line is only 24\,km\,s$^{-1}$, decreasing to 22\,km~s$^{-1}$ if the adopted 0.15845\,d
period is used to fit the data. The RMS is 16\,km~s$^{-1}$.

\begin{figure}
\setlength{\unitlength}{1mm}
\resizebox{15.cm}{!}{
\begin{picture}(130,105) (0,0)
\put(0,0) {\includegraphics[width=13cm, bb=0 500 390 820, clip=]{Fig8-bg.eps}}
\end{picture}}
\caption{The Doppler map of He I $\lambda5875.6$\,\AA\ emission. The trailed spectrum and reconstructed trailed spectrum of
the emission are presented in the bottom and the velocity map on top panel.
The Keplerian velocity of the disc in the Doppler maps is located at $ \upsilon_{\mathrm {disc}}\sin (i) \ge 220$\,km\,s$^{-1}$ and the circle
shows the disc external radius. The system parameters discussed in the text.}
\label{fig:tomohei}
\end{figure}

Armed with a set of two components comprising  H$\alpha$,   we may try to figure out their origin.
We compare our spectroscopic observation with a small sample of similar objects published recently
\citep{2017MNRAS.464..104H,2017MNRAS.470.1960H}, which show  similar two-component emission lines.
RW\,Sex and 1RXS\,J064434.5+334451 \citep{2017MNRAS.470.1960H} and  RW\, Tri \citep{Subebekova20} were all observed with the same instrumental
settings as BG\,Tri, so the measurements are uniform, and the comparison is straightforward. All three objects show two distinct components
varying with the respective orbital periods in almost counter-phase, relative to one another. One component is usually wider.
Another, the narrow one, is firmly linked to the irradiated face of the secondary by two eclipsing objects in the sample, for which the zero
phases were known precisely.
The wide component is also regularly the higher velocity component in other NLs. In case of BG\,Tri, the difference in widths of components is
insignificant, but still, the HVC is slightly broader than LVC (average FWHM$=5.7(8)$\,\AA\ vs $5.3(4)$\,\AA,  respectively).

Assuming that the secondary star emits the LVC, in analogy with the above-mentioned NLs \citep{2017MNRAS.470.1960H,Subebekova20}, we determine the orbital phase zero ($\upvarphi=0$)
of the system as the moment when the RV of LVC changes sign from negative to positive, i.e. when the secondary star is in the inferior
conjunction. In which case, the ephemeris  of BG\,Tri\ can be expressed as
\begin{equation}
 \mathrm{HJD_{\upvarphi=0}} = 245 8053.45490(60) + 0\fd15845(10)\times\mathrm{E}.
 \end{equation}
All phases used in this paper were calculated with this ephemeris.

\begin{figure*}
\setlength{\unitlength}{1mm}
\resizebox{15.cm}{!}{
\begin{picture}(130,100)(0,0)
\put(-10,0) {\includegraphics[width=15cm, bb=35 95 530 430, angle=0, clip]{Fig9-bg.eps}}
\end{picture}}
\caption{The geometric model of BG Tri.  The center of mass (x) and Lagrangian corresponding points are marked.  Velocities of the  L$_1$ point,  the disc outflow area (green), and the WD are denoted. LVC which is emitted from the irradiated hemisphere of the secondary star has a velocity exceeding that of the L$_1$ point and less than the orbital velocity of the star.}
\label{fig:Model}
\end{figure*}

\subsection{Doppler tomography}
\label{subsec:doptom}

A customary  way to illustrate the emission line behaviour is via trailed spectra and Doppler tomography \citep{1988MNRAS.235..269M}. It is
worth mentioning that the Doppler tomography works best if the emitting particles are in the orbital plane, and the inclination of the
system's orbital plane is high \citep{2005Ap&SS.296..403M}.
In order to construct trailed spectra and Doppler maps, we used the phase zero as defined above, stemming from the assumption
that the LVC is the component originating from the irradiated face of the secondary.
With this premise, the Doppler tomograms presented in Figures\,\ref{fig:tomo} and \ref{fig:tomohei} were constructed
\citep{1998astro.ph..6141S}. Echelle high-resolution spectra were used for this purpose.
 The Doppler map of the H$\alpha$ line without separation into two components was calculated, but is not presented here because it is less informative. Tomograms of unaltered lines were presented by \cite{2017MNRAS.470.1960H,2018ApJ...857...80G}. Instead,  we split the  H$\alpha$ line into components, as demonstrated in  the bottom panel of Figure\,\ref{fig:profiles}, and made a tomogram of each component separately.

In the bottom panels of Figure\,\ref{fig:tomo} trailed spectra (and their reconstructed counterparts) of
H$\alpha$'s  HVC and LVC are presented side by side. Together, they form
the trailed spectra of H$\alpha$ shown at the right side of Figure\,\ref{fig:rvcurves}.  Meanwhile,  in the upper panels, the velocity maps
resulting from the Doppler tomography are shown.  Locations of the
stellar components are marked by "$\times$", the centre of the masses by "$+$". The Roche lobe of the secondary star and the
ballistic trajectory of mass transfer flow are over-plotted, as well as a ring corresponding to
the outer radius of the disc. To calculate them, we selected the mass of the WD, M$_{\mathrm{WD}}=0.8$\,M$_{\sun}$, and the mass
ratio,  $q=0.4$\  as statistically average values for a P$_{\mathrm {orb}}=3.8$\,h nova-like CV
\citep{2011ApJS..194...28K,2011A&A...536A..42Z}.
The orbital inclination angle was fixed at  $i=25$$^\circ$\ (see Section\,\ref{systempar} for justification of these parameters).

The LVC produces a spot converging with the position of the secondary in the velocity map. Apparently, this is a result of our phase
allocation. Usually, when the irradiated secondary star forms the emission, the line is narrower  (3.8\,\AA\ in the eclipsing RW\,Tri
\citep{Subebekova20} against 5.3\,\AA\ in BG\,Tri), and the compact spot is concentrated at the hemisphere facing the WD. The reason for such a
diffuse spot is not clear, but a low orbital inclination of the system probably contributes to it.
Meanwhile, the HVC produces another diffuse  and elongated concentration (upper left panel), at a region which is clearly evading
identification with either the stellar component of the binary, the accretion disc, or the mass transfer stream; including impact area of the
stream with the disc. Detection of this H$\alpha$ component and its corresponding location in the velocity maps has become common for
RW\,Sex-type NLs. Among a few possible explanations cited by \citet{2017MNRAS.470.1960H} and \citet{Subebekova20}, we prefer the
model in which the outflow from the disc takes places in the orbital plane, instead of the wind perpendicular to the plane direction. Three-dimensional numerical simulations of the gas dynamics show that such outflows are viable through the vicinity of the Lagrange L$_3$ point \citep{2007ARep...51..836S}. BG\,Tri\ provides a good argument in favour of this hypothesis: firstly, the object shows meagre emission from \ion{He}{ii} line, even though we observe it almost face-on, hence it is difficult to argue that a disc wind
is significant enough to produce an intense enough emission spectrum \citep[e.g.][]{10.1093/mnras/stv867}  to overcome the bright accretion
disc. Generally, P\,Cygni-like profiles for NLs are observed in UV, and quite successfully modelled for recombination emission
\citep{2002ApJ...579..725L}, where the lines of low inclination systems  exhibit the characteristic imprint. However, reproducing it in the
optical range is a challenging task; it produces some double-peaked emission line contribution only in a high inclination ($i>60^\circ$) systems.
\citet{2016PhDT.......348M} attempted to convert lines into the single peaked, requiring an extension of the line forming region to $\sim$150
R$_{\mathrm {WD}}$, which again works only for high inclinations. As a result, \citet{2016PhDT.......348M} succeeded to produce a successful
model for RW\,Tri by comparing it to a low-resolution spectrum of the object. But \citet{Subebekova20} demonstrated that the H$\alpha$ in RW\,Tri
is complex and at least partially formed at the heated surface of the secondary star.
Secondly,  H$\alpha$ emission has been disentangled already in four objects, including BG\,Tri,  all of which have vastly different inclination
angles. After correction for the inclination angle $i=25$$^\circ$ (see Section\,\ref{systempar}),  the measured $\upsilon_{\mathrm{HVC}}/
\sin(i)=121$\,km~s$^{-1}$ of the HVC  converts into  286~km~s$^{-1}$. According to \citet{2017MNRAS.470.1960H} and \citet{Subebekova20} the
HVC  (also called "the wide component" in these publications) in all studied objects is $\approx300$\,km~s$^{-1}$, after the inclination angle
is accounted for.
The fact that the HVC in all morphologically similar NL variables obtains the same value  after correction for a variety of inclination
angles, is a good evidence that the source of HVC is in the orbital plane.
One would expect that the wind will constitute itself  differently, depending on the viewing aspect.  Notwithstanding, the HVC always appears on the
Doppler maps at the same spot, adjacent to the outer edge of the accretion disc on the opposite side from the secondary/hot-spot,
regardless of the system inclination.

Figure\,\ref{fig:lines} demonstrates that \ion{He}{i} acts somewhat differently with respect to the Balmer lines. It is also a common
characteristic of RW\,Sex-type NLs.
Helium lines are  fainter than H$\alpha$ or H$\beta$ and are comprised of equally intense emission and absorption. Nevertheless, we explored
their phase evolution using illustrative trailed spectra and their respective tomograms. We concentrated on the \ion{He}{i}
$\lambda\,5875.6$\,\AA\ line, which has the best S/N among helium lines. A trailed and reconstructed spectra of the emission component of this  line,  and the corresponding tomogram
is presented in
Figure\,\ref{fig:tomohei}. Meanwhile, the same line is treated as an absorption feature  on the right side.
The emission component of the line basically repeats the pattern observed in H$\alpha$. The observed trailed spectrum is faint, but the
program picks up the signal correctly, reflecting it in the reconstructed spectrum. The low-velocity component definitely dominates, and hence
a compact spot materialises  close to the L$_1$ point, contrary to the diffuse appearance in the  H$\alpha$ case. The HVC is hardly traceable
in the observed trailed spectra, but apparently some emission comes from here too. Hence, a coma-like extension in the velocity map.

\begin{figure}
\setlength{\unitlength}{1mm}
\resizebox{15.cm}{!}{
\begin{picture}(130,55)(0,0)
\put(0,0) {\includegraphics[width=7.25cm, bb=15 200 585 630, clip=]{Fig10-bg.eps}}
\end{picture}}
\caption{
 The plot of spectral energy distribution of BG\,Tri\ in the bottom panel. Circles represent the fluxes from
 Table\,\ref{tab:SEDlog}. They were corrected for the interstellar extinction E($B-V$)=0.03.
 The dashed line through the observed data in the optical-IR range  represents the spectrum of accretion disc.
 The red points represent a spectrum of a M3V star scaled to  a 337\,pc distance.
 The solid line is a combination of fluxes from the accretion disc and the secondary. The outermost left two points correspond to UV data.
 In the upper panel the best fit parameters (mass accretion rate vs. inclination angle) of the accretion disc model to the data are presented
 in the form of intensity map. The extreme boundaries of $i$ corresponding to the secondary mass center and L$_1$ point are marked by
 vertical lines. Preferred values of $\dot M$ and $i$ (blue strip) are also function of increasing surface and decreasing temperature along
 latitude. }
\label{fig:sed}
\end{figure}

\section{SYSTEM PARAMETERS}
\label{systempar}

The average masses of WDs in CVs   above the period gap is M$_{\mathrm{wd}}$(P$_{\mathrm{orb}} > 3$ h) $= 0.86(20)$ M$_{\sun}$\
\citep{2011A&A...536A..42Z}.
For simplicity, we adopted  M$_{\mathrm{WD}}=0.8$\,M$_{\sun}$. Taking into account the semi-empiric relation of secondary type vs orbital period, we
expect a secondary with a mass of M$_2\approx 0.3$\,M$_{\sun}$, and spectral type of M3V-M4V \citep{2006MNRAS.373..484K}. The expected mass ratio
and separations are $q \equiv {\mathrm{M}}_2/{\mathrm{M}}_{\mathrm{WD}}\approx0.4$ and $a=1.23$\,R$_{\sun}$, respectively. The  accretion disc
truncation radius\footnote{equation 2.61 from \citet{1995CAS....28.....W}} is $r_{\mathrm{disc}}^{\mathrm{out}} = 0.52$\,R$_{\sun}$.
Corresponding primary, secondary, and L$_1$ orbital velocities are 117\,km s$^{-1}$,  292\,km\,s$^{-1}$, and  129\,km\,s$^{-1}$, respectively (see
Figure~\ref{fig:Model}).

 There are numerous flux measurements of BG\,Tri\ available  in the public domain. We fetched all available data from
 VizieR\footnote{http://vizier.unistra.fr/vizier/sed/} \citep{2000A&AS..143...23O}.
 We revised the available data, since some measurements are erroneous  (e.g. the SDSS data are not correct because the object is too bright),
 and  compiled those which passed the scrutiny in Table\,\ref{tab:SEDlog}.
Selected data are plotted using  circles in the bottom panel of Figure~\ref{fig:sed}, after the interstellar reddening correction
of E($B-V$)=0.03 \citep{2015ApJ...810...25G}.
Using the  {\it Gaia} distance of $d= 334(8)$\,pc, we can calculate the luminosity of different components.
In particular, even a hot 50\,kK white dwarf will have a negligible contribution to the optical flux. A secondary M3-4\,V Roche lobe filling
star has some insignificant influence in the IR. The comparison of the observed fluxes with those expected from different components confirms that
the flux in the entire wavelength range  is formed mostly by the accretion disc.
The dashed lines in the bottom panel of Figure~\ref{fig:sed} indicate a simple accretion disc spectrum as a composition of multiple
black-bodies; from concentric rings with a corresponding distribution of temperatures throughout the stationary, optically thick disc
\citep{1989A&A...211..131L}. Since the observed flux would depend on the aspect of the disc, we fitted the observed SED as a function of the
mass transfer rate $\dot M$, and  the system inclination.

The UV points were excluded from consideration because  it is well known that accretion disc models do not reproduce  the observed spectrum
shape of CVs in the wide range including the UV \citep{2007AJ....134.1923P}.

For the fit's robustness, we added a  spectrum of  M3V-type stars from the empirical template library of the Sloan Digital Sky Survey stellar
spectra \citep{Kesseli:2017aa}, which was extended to the IR range using  spectral templates from \citet{Rayner:2009aa}.
The star spectrum was scaled to the object's distance.  For each band listed in Table\,\ref{tab:SEDlog} (except $FUV$ and $NUV$) the flux $m_{calc}$ was calculated as a sum of the disc model and the secondary.
The result of the best fit of function $\chi^2 = \Sigma ((m_{obs} - m_{calc})/\Delta m_{obs})^2$ is presented as a long dashed line in the
lower panel of  Figure\,\ref{fig:sed}.
In the upper panel of  Figure\,\ref{fig:sed}, the goodness-of-fit is presented as an intensity scale diagram.
Following the assumption that the LVC is emitted from the heated hemisphere of the companion star, the expected LVC velocity is located in the
range of  $\upsilon_{\mathrm{LVC}} \in $  [130\,$\sin(i), 290\,\sin(i)$\,km~s$^{-1}$] (see Figure\,\ref{fig:Model}), which allow us to estimate
limits on the orbit inclination from the dynamical constrains.  The observed value of LVC is 78\,km~s$^{-1}$, which defines the limits marked by
the vertical dashed lines in  Figure\,\ref{fig:sed}, top.
The line at the right side of the plot indicates the observed LVC, which is consistent with the L$_1$ point, and another corresponds to the center of
mass of the secondary (at the left side). In other words, the inclination angle and mass accretion rate would be highest if the LVC is
emitted just from the  L$_1$ point, and accordingly, lowest if the entire surface of the secondary is heated. Of course, neither
assumption is correct,
so we introduced some parameter which reflects the increasing cross-section of the secondary, with decreasing temperature. According to which,
the best fit is achieved  at $i=25(5)$\,degree and $\dot M$=$8.0(1.0)\times10^{-9}$\,M$_{\sun}$\,year$^{-1}$.

Given all uncertainties of adopted assumptions, the fit is remarkably good. The values of mass accretion rate are within the range of
estimates for a number of other NLs \citep[e.g. Figure 2 of ][]{2019arXiv191001852H}.  The mass transfer $\dot M$\  dependends slightly on
the mass of the WD. For a 0.6\,M$_{\sun}$ WD,  the mass transfer rate  increases to  10$^{-8}$\,M$_{\sun}$\,year$^{-1}$. On the down side,   $\dot M$\  is
$\sim4.0\times10^{-9}$\,M$_{\sun}$\,year$^{-1}$  for a massive $\geq1.0$\,M$_{\sun}$\ WD.

 The LVC velocity corrected for a system inclination of  $i=25$\,$^\circ$\  is $\upsilon_{\mathrm{LVC}} =$ 185\,km~s$^{-1}$.
As we showed earlier, the corrected HVC velocity is $\approx300$\,km~s$^{-1}$,   it corresponds to the orbital velocity at the edge of the disc on the opposing side of the system relative to the secondary.
The location of the HVC on Doppler maps of all similar NLs is related to the Lagrangean  L$_3$ point. According to some hydrodynamic models
\citep[]{2007ARep...51..836S, 2017MNRAS.467.2934L}
an outflow of matter from the disc  in to the orbital plane takes place from this area (marked green area in
Figure\,\ref{fig:Model}). The concentration of gas in that area might be responsible for HVC or wide component of emission lines in these
objects.

\begin{table}

\caption{VizieR photometric data of BG Tri}
\label{tab:SEDlog}
\begin{tabular}{cccccc}
  \hline \hline
$\lambda$  & Flux & 1$\sigma$ Flux & Band & Source & Ref. \\
($\mu$m)  & ($\times 10^{-3}$Jy)  & $\times 10^{-3}$   &    &  &   \\ \hline
0.153 & 32.1 &0.2  & $FUV$ & \textit{GALEX} & 1 \\
0.231 & 19.3 &0.1  & $NUV$ & \textit{GALEX} & 1\\
0.444 & 64.2 &	11.6	& :B & AAVSO  & 2 \\
0.477 & 79.0 & 	    & $g$  & PAN-STARRS & 3 \\
0.482 & 64.6 &	9.3 &	$g'$ & AAVSO & 2 \\
0.505 & 65.7 & 0.9 & $Gbp$ & \textit{GAIA2} & 4 \\
0.554 & 61.4  & 9.6 & $V$ &	AAVSO & 2 \\
0.613 & 63.2 & 	   & $r$ & PAN-STARRS & 3 \\
0.623 & 58.9 & 0.3 & $G$ & \textit{GAIA2} & 4 \\
0.625 & 58.7 &	7.7& $r'$ &	AAVSO & 2 \\
0.748 & 51.6 & 	   & $i$ & PAN-STARRS & 3 \\
0.763 & 51.5 &	7.6 &	$i'$ & AAVSO & 2 \\
0.772 & 49.6 & 0.7 & $Grp$  & \textit{GAIA2} & 4 \\
0.865 & 44.2 & 	   & $z$ & PAN-STARRS & 3 \\
0.960 & 36.5 & 0.8& $y$ & PAN-STARRS: & 3 \\
1.24 & 29.9 &0.6 & $J$ & 2MASS & 5\\
1.65 & 20.6 &0.4 & $H$ & 2MASS & 5\\
2.16 & 14.0 &0.2 & $Ks$ & 2MASS & 5 \\
3.35 & 6.85 &0.15 &$W1$ &  \textit{WISE} & 6\\
4.60 & 4.19 &0.08 & $W2$ &  \textit{WISE} & 6 \\
1.16 & 0.89 &0.09 & $W3$ &  \textit{WISE} & 6 \\
 \hline
\end{tabular}
\begin{tabular}{l}
1 - \citet{2017ApJS..230...24B} \\
2 - \citet{2015AAS...22533616H} \\
3 - \citet{2016arXiv161205560C} \\
4 - \citet{2018AA...616A...1G} \\
5 - \citet{2003yCat.2246....0C} \\
6 - \cite{2012yCat.2311....0C} \\
\end{tabular}
\end{table}

\section{Conclusions}
\label{sec:conclusions}

We studied BG\,Tri, one of the brightest CVs at $V=11.9$, which somehow escaped attention until now. We determined its orbital period to be
0.15845\,d or 3.8028\,h.  We show that it is a  NL system, identified by its characteristic blue spectrum containing a set of \ion{H}{i} and
\ion{He}{i} lines, comprised of wide absorption features containing strong emission peaks. The orbital period and the spectrum, combined with
the SED, indicate the presence of a bright accretion disc in a high density and temperature state, proper to NLs. The long term light curve of
BG\,Tri, obtained by ASAS\,SN and CRTS sky surveys, shows the absence of dwarf novae style outbursts, but reveals an instance of low luminosity
state often detected in NLs, also known as the VY\,Scl phenomenon.

 Absorption lines originate from the optically thick accretion disc, while emission forms elsewhere.  We demonstrate that the Balmer emission
lines are complex and we are able to separate H$\alpha$ into two components.
We identify the LVC with the heated surface of the secondary star facing the luminous disc.
We associate the HVC  with the disc outflow region situated on the opposite from the
secondary and the hot-spot, side of the disc. A similar occurrence is also common for mentioned NLs, which we may call RW\,Sex type systems, all of which are concentrated in a 3-6\,h range of orbital periods \citep{Subebekova20}.
An HVC velocity, corrected for the inclination angle, of $\sim$300\,km sec$^{-1}$, is very definite in all studied objects, regardless of their
orientation. That, in our opinion, argues against the disc wind origin of the HVC component. However, it is not evidence of the absence of wind,
just a rationalisation that emission lines in the optical range are not formed in the wind.

The SED of BG\,Tri\ confirms that stellar components contribution is negligible and that most of the flux from UV to  near-IR is emitted by the
disc. The energy balance favours  that we observe the system nearly face-on, and the deduced inclination angle validates the value fetched
from the dynamical considerations.

\section*{Acknowledgements}

 We are grateful to the anonymous referee for the valuable comments which helped to improve this paper. This work is based upon observations carried out at the OAN SPM, Baja California, M\'{e}xico. We thank the daytime and night support staff at the OAN-SPM for facilitating and helping obtain our observations. This research has made use of the VizieR catalogue access tool, CDS, Strasbourg, France (DOI: 10.26093/cds/vizier). The original description of the VizieR service was published in A\&AS 143, 23.
GT and SZ acknowledge PAPIIT-DGAPA-UNAM (grants IN108316, IN102120 and IN110619) and CONACyT grant 166376.  MSH acknowledges the Fellowship for National PhD from ANID, grant number 21170070. MSH and GT are thankful to SIMA project 687 of UNAM.   This research has been was funded in a part by the Science Committee of the Ministry of Education and Science of the Republic of Kazakhstan (Grant No. AP08856419).
BTG was supported by a Leverhulme Research Fellowship and the UK STFC grant ST/T000406/1. AA received support from Thailand Science Research and Innovation (TSRI) grant FRB640025 contract no. R2564B006.

\section*{Data Availability}
The data underlying this article will be shared on reasonable request to the corresponding author.

\bibliographystyle{mnras}

redpajama_set_name: RedPajamaArXiv


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Mo Bro's wins the Leicester Mercury Retail Award of the year!
We are happy to announce that on Thursday 12th April at the Leicester Mercury Business Awards we won the 'Retail Business Of The Year' award!


My current position as Director for Initial Teacher Training (FE and Skills) at the University of Warwick, requires me to quality assure and quality improve teacher training provision across 7 General Further Education Colleges in the Midlands. Prior to this I worked in further education for 23 years. My teaching career started in 1991. I quickly moved in to a full time teaching role and not long afterwards in to educational management. My last role was as Head of Centre for Daventry, which is one of three main sites at Northampton College. This was a strategic role requiring me to effectively lead on matters relating to estates and facilities and to liaise with appropriate personnel on all aspects of the curriculum and the quality of provision thereafter. I was also the advisor on education matters in local strategic partnerships and other external committees. Prior to this I worked as Director for Business and Management at North Warwickshire and Hinckley College strategically leading and operationally managing a wide range of curriculum areas including Business and Management, Computing, Access to Higher Education, Maths and English GCSE provision and Initial Teacher Education. I have two grown up children, my daughter is a primary school teacher and my son is a motor vehicle mechanic.


Send in your CV questions!
We all know writing a CV or choosing a CV writer can be difficult, so we would like to assist you by answering your CV-related questions.
The best question is published on the CVclinique website at the end of each month.


WWE Mayhem – cool sports action about the world of wrestling. The game has beautiful graphics, convenient control, a large set of actions, strikes and receptions, the ability to act in the ring as one of the famous and recognizable fighters, and much more, which makes this fighting game so popular and stands out among the others. Well, constant updates, additions and improvements do not let even the most demanding gamers get bored.


text:
Press, Etc.
Bottom Of The Barrel- Matt Benevoli
Bottom Of The Barrel- Rod Redford
Bottom Of The Barrel- Mike Shum
The Bartender's List
The Bartender's List- Jeffrey Morgenthaler (2.0)
The Bartender's List- Alejandro De La Parra
The Bartender's List- Jasmine Radu
The Analog Hour- Second Hand News
Brandied Cherries
Drinks With A View- Sidecut at Four Seasons Resort Whistler
Small Batch- Camper Cocktails
Small Batch- Travis Fourmont
Small Batch- The Commissary
COTD
Cocktail Of The Day- The Cherry Blossom
Cocktail Of The Day- Birds and the Bees
Cocktail Of The Day- The Rainmaker
By Two for the Bar The Bartender's List November 13, 2014
The Bartender's List- Jeffrey Morgenthaler
So I know I had retired The Bartender's List a few weeks ago as it was intended to be a summer series. And the fact that it is now dark at 4:30pm suggests we are well into fall. But sometimes you just have to bring a good thing out of retirement. Especially when someone like Jeffrey Morgenthaler begs you to do an interview with him…. I may have the details wrong on that one. But whatever. The details are secondary. Point is, someone begged someone for an interview and someone said yes and the other someone had an excitement-induced panic attack.
For those that don't know who the man is, here's the Cole's Notes: Jeffrey Morgenthaler. The Bar Book. Clyde Common. Pepe Le Moko. Playboy Magazine (columnist, not centerfold…..that I know of). Grandaddy of the barrel aged cocktail. A quick google search will tell you that he is a highly accomplished and well-respected bartender.
But when you sit at Jeffrey's bar, the magnitude of his achievements aren't really in the foreground. It's not that you're not aware of them. His talent and success as a bartender is always clear, but when you are sitting in front of him having a conversation over one of his creations, Jeffrey just becomes a guy. He's sarcastic, opinionated, crass and kinda loud. It's clear that he takes what he does seriously but self-deprecating humour is very much a part of his repertoire.
Perhaps you'd imagine that sitting at his bar would involve a discussion about obscure cocktail recipes or long-lost ingredients. And I'm sure that happens. But that last time I sat across from Jeffrey, we had an in-depth conversation on the merits of Kelly Kapowski over one of the finest whiskey sours I've ever had. And that was just fine by me.
I went to Portland this past weekend to photograph for this article. On my way out of the Clyde, Jeffrey rather sarcastically said "I look forward to your scathing exposé." Well, here you have it. I wouldn't call it scathing, but it's most definitely unedited, unabridged, unadulterated Jeffrey Morgenthaler at his finest.
1) What was your first sip of alcohol?
Oddly enough it was scotch whisky. I don't remember which brand it was, but I remember that it looked pretty fancy. I was in high school and really loved the Beatles. I mean, they weren't a group when I was in high school, let's just get that straight. Anyway, I read that they drank scotch and Coke, and so I tried one. My parents had a lot of it in the liquor cabinet.
2) If you could only have a 5 bottle bar, what would they be?
One bottle of London dry gin, one bottle of really fucking nice silver tequila, and three bottles of cask strength Islay whisky.
3) What is your death-row drink?
Like, I'm on death row and they're going to let me have one drink before they kill me? Is that what this question means? I mean, if I'm about to be killed, I guess I'd request a pint glass full of vodka. What do other people say to this question, like they'd want to sip on a Remember the Maine right before they get electrocuted? Fuck that. They can carry my black-out drunk ass to the chair.
4) Was there anything that you really wanted in your book that didn't make the final cut?
I really wanted the whole thing to be illustrated. Tons of illustrations, sidebars with recommended tools, all that. But my publisher was like, no, we're going to do photos. Fortunately Alanna is an incredible photographer and the book turned out great.
5) The album that captures the feel of your dream bar?
That changes often. Back when I was working in dive bars it was Small Change by Tom Waits. I think that's the anthem album to pretty much every dive bar out there. Now, I don't know. Know the soundtrack to Breakfast at Tiffany's? The one by Henry Mancini? I think that sounds like a pretty classy bar.
6) The one cocktail book that should be behind every the bar?
Mine. No, just kidding. Honestly, you need a book that's got great recipes that you can trust. It's hard finding one book that's good all around. I think Jim's PDT Book is super reliable.
7) The one non-cocktail book that should be behind every bar?
The Guinness Book of World Records. That's what it's for.
8) Most unusual drink request?
We had a regular down in Eugene who would come in after work every day and have – ready for this? A Beefeater gin and Pepsi. I've heard of some weird drinks, but that is seriously fucked up. Gin and Pepsi? That's like what you make when you're under age and don't know any better. But you don't go around being a grown-ass man drinking that shit. This guy was like 50. I'll bet he'd been drinking them since he was 11.
9) If you could make a cocktail for anybody, dead or alive, who would it be and what would you make them?
I want to make a drink for the President. Doesn't matter who it is at the time. I think that's the top, when you go to the White House and make a cocktail for the president. That's when you're like officially the best bartender in America.
10) On nights when you're totally in the weeds, what makes it worth being behind the bar?
Pretty girls. Oh, and money. Those are the only two reasons I got into this miserable line of work in the first place. I never wanted to be a bartender for the rest of my life – who on earth would? Standing on your feet for ten hours a day, listening to drunk people babble on, cleaning up puke and stuff. No, babes and cash. That's what it's all about.
11) The menu at Pepe seems to embrace a more maligned variety of cocktail like the Amaretto Sour and a shamrock green Grasshopper (which a lot of craft bartenders tend to shy away from). What is something your peers have embraced that you just can't get behind?
Uh, probably a menu full of brown, bitter, and stirred drinks with ingredients even I have never heard of. That's something I can't get behind. When did you guys all get together and decide to make drinking in bars a really miserable experience? Because I missed that meeting. I'm not saying you need a menu full of dumb drinks like mine, but for the love of god, please stop it with this shit.
12) If your shifts behind the bar had a theme song, what would it be?
Carmina Burana. Just kidding. It would be like Baby Elephant Walk or something. Henry Mancini! I didn't think I really liked his music but apparently it's my theme music.
13) Best bar fight you've ever witnessed- GO!
I went to a regular haunt one night after work. It was kind of a fancy place. Anyway, I'm standing next to this weird dude. Young kid. I pay for my drink and leave a big tip, and this kid started telling me what a good tip that was, and how it's really important to tip your bartender. I'm like, yeah yeah, please stop talking. Anyway, he's super weird – I'm guessing meth, since this was in Eugene. So he's really bugging me, still talking about tipping. He tells me that he works in a gas station, and that every day this old man comes in and gets like a newspaper or whatever, and gives this kid $20 and says "Keep the change".
And I'm like, increasingly getting annoyed with this kid. So I tell him, "I hate to break it to you, but that old man is only doing that because he wants to get in your pants."
Oops. With one punch to the chest, this kid laid me out flat on the floor. I wasn't even mad, I thought it was hilarious. But instead of coming over and kicking my ass, as he was hoping to do, the entire bar jumped on this kid and literally threw him out onto the street. And he's looking at me through the window, and I'm thinking, "Sorry man, I guess I should have told you that I'm pretty much the favorite regular here."
14) Other than the recent incident with the finger, what is the worst injury you've endured behind the bar?
Why is my finger injury so well known? I was in Berlin a couple of weeks ago, and people I didn't even know were like, "How's the finger healing?" I took my fingernail off with a vegetable peeler, which was really horrible, but there's like this Save Ferris thing happening. Still. When I was in LA, all the bartenders were bandaging their ring fingers in solidarity. I'm like, what is going on here. But yeah, that was probably my worst injury.
15) First bar you were ever thrown out of? Last bar you were ever thrown out of?
I've never been thrown out of a bar.
16) What is your favourite fictional bar from tv, movie or book?
Cheers. All the way.
17) What is the most enticing opportunity you've ever turned down?
I don't really turn down a lot of good opportunities. If it seems like it's good for my career and something I actually want to be associated with, I'll do it. I want to contribute as much as I can to this industry, so I welcome anything that enables me to do that. The book was like that. I wasn't actively seeking to write a book, but the opportunity came to me and I used it to contribute something I feel is valuable to the business. That's why it's not the Big Book of Jeffrey Morgenthaler's Cocktail Recipes. Because I didn't think that would be valuable.
18) What is your favourite three-ingredient cocktail and how do you make it?
A Daiquiri.
Check out the "How to Not F@%& Up a Daiquiri" on Small Screen for Jeff's recipe.
Previous articleThe Bartender's List- Thor Paulson
Next articleThe Bartender's List- Jim Meehan
Portland Cocktail Week- Bon Vivants Volunteer Day
The bartending community is descending upon Portland in droves as the city's annual Cocktail Week kicks off. From green bartenders to seasoned veterans, the…
© Two for the Bar. All rights reserved.

redpajama_set_name: RedPajamaCommonCrawl


James is a lawyer who represents injured workers throughout Illinois. He received his law degree from John Marshal School of Law, and established the law firm of Marszalek and Marszalek. James is active in various legal organizations, and is a frequent lecturer/guest speaker at University of Illinois Law School, and various unions throughout Illinois.


text:
Digital tax
Luxembourg will lose out from global tax overhaul, OECD chief says
Amazon would likely pay less tax in the Grand Duchy, says Pascal Saint-Amans
Hannah Brenton
Luxembourg will be one of the losers from a global tax reform that revamps where technology giants like Facebook and Amazon pay taxes, the chief architect of the overhaul says.
Pascal Saint-Amans, who heads the tax division at the Organisation for Economic Cooperation and Development (OECD), is spearheading an international effort to rework global tax rules for the digital age.


Thank you for your interest in registering for the GM Enthusiast Network and gmdelta.com. Your FREE registration on this site will give you access to any and all GM Enthusiast Network sites!
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IF YOU DO NOT ACCURATELY ENTER YOUR EMAIL ADDRESS THEN YOUR ACCOUNT WILL NOT BE ACTIVATED! When you complete registration an email is sent to the address you specify. You will need to read that email and follow the instructions in it. If this email bounces, your account will be automatically deleted.
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The Tri-Fold Golf Towels make an excellent addition to any golfer's bag. These towels are 100% cotton terry cloth that comes with a grommet and bag clip to attach easily to any golfer's bag.
This package contains 2 Golf Towels. Always have a spare.
TRI-FOLD ABSORBENT: Extra large 16" x 25", helps you clean up well. This superb golfing accessory allows you to keep your equipment clean and free from dirt.
A BLACK TRI - FOLD GOLF TOWEL looks professional, which is exactly what you want when you're out on the Golf Course.
THESE PREMIUM QUALITY golf towels are made of 100% cotton terry-cloth, high quality and durable.
THE GROMMETS on our black terry velour golf towels are sturdy, and will securely hold your golf towel to your bag.
THE CARABINEER CLIP and metal gromment attachment can easily attach around anything such as your bag, cart, or your push cart. These towels also work great for fisherman. Just clip them on your boat and clean the hands after catching your fish.
If you have any questions about this product by Show Car Guys, contact us by completing and submitting the form below. If you are looking for a specif part number, please include it with your message.


Dr. T & Guess Who?
Wilma Taylor Ministries is a 501c3 organization that services youth, families and senior citizens by developing leaders to serve humanity. This is done through workshops, seminar and the presentation of special services. Wilma Taylor Ministries is also geared to promoting the development of music through training and educational series presentations. The goal of Wilma Taylor Ministries is to enable others to develop their talents and serve their communities at large.
Click on this picture for more..
Dr. T and Guess Who?
Recently, Dr. Wilma Taylor attended a very important event.
Click this link to view pictures Dr. T & Guess Who?
There is a chinese proverb that says "Give a man a fish and he can eat for a day. Teach a man to fish and he can eat for a lifetime.": I have found this proverb to be particularly true and the mission of Wilma Taylor Ministries is to empower others so that they can survive on their own and pass this skill on.
Copyright by Wilma Taylor Ministries, July 2009 - Website Designer; Phoenixzone Graphix, Inc.


After the close on Dec. 29, Innocoll Holdings announced that it received a Refusal to File letter from the Food and Drug Administration for XaraColl new drug application (NDA).
As a reminder, Innocoll (ticker: INNL) is developing XaraColl for the treatment of post-surgical pain. Upon preliminary review, the FDA determined that the application was incomplete to permit a substantive review.
In the letter, the FDA stated that XaraColl should be characterized as a drug/device combination, which would require Innocoll to submit additional information to the FDA. The next steps involve requesting a Type A meeting with the FDA, where the company will seek additional clarification of what information, if any, will be required. Innocoll will disclose additional details in the future after discussions with the FDA.
We are stepping to the sidelines due to the ambiguity in timelines and are downgrading the stock to Market Perform from Outperform.
In addition to downgrading the stock, we are also lowering our price target to $2 from $10 as we have pushed out the approval timeline for XaraColl and lowered our probability of approval.
We believe the company needs to raise additional funds in early 2017 to support the regulatory filing for XaraColl, including potential additional data gathering, and the potential commercialization of the product.
We are raising our fourth-quarter non-GAAP earnings-per-share estimate to a loss of 37 cents from a loss of 39 cents due to lower expense expectations. In addition, we are increasing our fiscal 2016 and 2017 non-GAAP EPS estimates to losses of $2.33 and 27 cents, respectively, from losses of $2.35 and $1.11, respectively, due to lower expense expectations and a higher share count.


Allgemeine geographische Ephemeriden. Bd.1(1789)-Bd.9(1802),Bd.11(1803)-Bd.28(1808),Bd.30(1809),Bd.33(1810)-Bd.51(1816)Issues missing.
The Astrophysical journal. v.1-v.437(1895-1997)Vols. 82,86,121-123 incomplete.
Engineering and science series / n.d.
A Previsão do tempo. v.6(1944),v.18(1955)-v.22(1959)Issues missing.
Proceedings of the National Academy of Sciences of the United States of America. v.1-v.3(1915-1917)Issues missing.
Publicationen der v. Kuffner'schen Sternwarte. 1889-1912?


TheMoneyIllusion » I'd really like to retire, but . . .
I'd really like to retire, but . . .
BRUSSELS – Interest rates are now close to zero throughout the developed world (the United States, Europe, and Japan). But the global economy is slowing down, and financial markets went into a tailspin during the summer. This suggests that the problem is more profound than one of insufficient monetary stimulus.
THAT is the problem we face.
This entry was posted on September 09th, 2011 and is filed under Monetary Theory. You can follow any responses to this entry through the RSS 2.0 feed. You can leave a response or Trackback from your own site.
Damn if we didn't elect John McCain president. I had a lot of fun back in early 2008 writing exam questions about his wish that interest rates were 0, but it doesn't seem quite so funny now, does it?
Seriously – Rogoff's book ("This Time It's Different") reports that there were various times (notably after the Tulip debacle) where real interest was so low that nobody could make a living on intermediated investment. So everybody had to be a "businessman" of some kind.
I find myself facing (more broadly and abstractly) this very issue.
I guess the question is, when will enough people go "start something" to fix the problem? How long do real interest rates have to be negative before cash looks for a better home?
MikeDC, If McCain were President now the GOP would be polling at sub-Herbert Hoover levels. They are soooo lucky.
Bryan, But the S&P earns nearly $100, on a level of 1100. That's a pretty good rate of return. Unless it goes down. . .
Russ, I'm guessing he didn't study monetary theory under Milton Friedman.
ChacoKevy, Yes, that's how I feel.
10 year German bond rates are even lower than the 10 year Treasuries. Both interest rate levels represent extremely "tight" (long-term), monetary policies.
Back during the Great Depression Congress failed to issue an adequate volume of goverment debt which the frbNY needed to "prime the pump". In this Great Recession, Bernanke introduced IOeRs to take Treasuries off the market & thus sterilize their purchases. But long-term growth rates for monetary flows (our means-of-payment money X's its transactions rate-of-turnover are still at sub-par rates-of-change realative to real-output. Bernanke's error slowed the current recovery.
When CBs grant loans to, or purchase securities from, the non-bank public, they acquire title to earning assets by initially, the creation of an equal volume of new money — somewhere in the banking system. I.e., commercial bank deposits are the result of lending, not the other way around.
Thus the expansion of commercial, MSB, CU, & S&L, bank credit (in the deposit taking, money creating, financial institutions), mirrors the growth in the stock of money. If bank credit (not Reserve bank credit), is growing, then so is the overall money supply.
The current shift by bank customers in their deposit classifications is just the reverse of shifts that occured in the high interest rate environment of the early 80's. Whereas then, DDs shrank & velocity increased, today the ratio of DDs has risen & the velocity of those deposits has declined.
The upshot is monetary policy is too restrictive and the rate-of-change in nominal gDp is too low.
That's a very good point about demand deposit velocity and interest rates. Another reason, incidentally, not to target M1.
May I ask where you get your figures for "means of payment money" and "transactions rate of turnover"? I'm assuming that the former isn't any particular monetary aggregate and the latter isn't real GDP.
flow5, I have the same general view, but I cut out the monetary aggregate middleman. I just focus on NGDP growth, which is too low. That means the Fed needs to do more regardless of where all the monetary aggregates are moving.
Professor: I guess that is equivalent to "dumbing it down" for Bernanke & co.
Joeseph Granville published his OBV, etc., & then his followers were able to anticipate his calls – thereby changing what the market turning point would have been. He is a great technical analyst but his record has been distorted because the market discounted his analysis.
Have you encountered the line of analysis given in this (http://www.hussmanfunds.com/wmc/wmc110124.htm) post?
The empirical relationships do seem to argue that there are substantial non-linearity and variability in the Fed's control linkages. If these real world effects are inescapable how does that affect your proposal for NGDP targeting?
Scott Sumner, you are pushing a "solution" that was proven to be unworkable by people who know how the Fed and the banking system works. Why do you push a dead idea that monetary stimulus would help? Your kind of stimulus (negative interest on reserves) was shown to be … contractionary. How much worse can it get?
No other group spues more lies than the MMT fraternity.
Tell me more. The rest of your post is very old MMT stuff, but this is interesting.
Read Wray, understand what reserves do and don't do and you will get it.
Hmmm, MMT lies? If this was so, SS wouldn't have to complain that it focuses too much on reality, LOL.
SS has nothing that could refute anything MMT says, not a thing.
There is nothing about negative interest rates on reserves in that article. It talks about POSITIVE interest rates on reserves a bit, though. Perhaps you meant that positive interest rates on reserves are contractionary, since they erode the difference between cash reserves and securities?
No, positive interest on reserves is actually expansionary. You are confused about basics as most of readers (and the author) of this blog. Read Wray, read Fullwiler, read Lavoie, read Moore.
So the erosion of the distinction between t-bills and cash as a result of IOER is expansionary?
"The erosion of distinction" has no effect. Short rate does and the interest income. Did you read the sources I guggested? You are fast.
Well, the first source you gave had absolutely nothing to do with the effects of negative interest rates on reserves and talked about something which you now say "has not effect". My interest waned after that point- I really was interested in have a debate about a situation where increasing the demand for base money had a contractionary effect, but apparentely I'm not getting that debate (right now).
* reducing the demand for base money.
MMT'ers were the last ones (not the only ones), to recognize that banks aren't reserve constrained, that banks don't loan out excess reserves, that loans create deposits, etc. Yes indeed, what a joke.
And MMT's sectoral balance equation doesn't balance. So much for reality.
D.F. Linton, Yes, many have shown me that article, but I'm afraid he makes a fundamental mistake. If the central bank is inflation targeting, then money supply changes will tend to be negatively correlated with V. But that says nothing about causality. It's why monetarist theories looked worse after the Fed got better at stabilizing NGDP.
OhMy, Reducing demand for the medium of account is expansionary. That's S&D 101. And have you checked out Sweden recently?
And as far as "read Wray" don't you know that Krugman, Rowe, DeLong, Beckworth, me, and everyone else has read Wray, Mosler, etc. We simply find their arguments wrong, and I've said why in many posts.


text:
"""Tests for DBObject.
"""

__author__ = 'andy@emailscrubbed.com (Andy Kimball)'

import json
import mock
import time
import unittest

from cStringIO import StringIO
from functools import partial
from tornado import httpclient
from viewfinder.backend.base.testing import MockAsyncHTTPClient
from viewfinder.backend.db import dynamodb_client, vf_schema
from viewfinder.backend.db.db_client import DBKey
from viewfinder.backend.db.episode import Episode
from viewfinder.backend.db.photo import Photo
from viewfinder.backend.db.post import Post
from viewfinder.backend.db.test.base_test import DBBaseTestCase

class DBObjectTestCase(DBBaseTestCase):
  @unittest.skip("needs aws credentials")
  def testRangeQuery(self):
    """Test DBRangeObject.RangeQuery."""
    def _MakeResponse(max_index, request):
      # Enforce maximum limit of 2.
      request_dict = json.loads(request.body)
      limit = min(request_dict.get('Limit', 2), 2)
      is_count = request_dict.get('Count')

      if 'ExclusiveStartKey' in request_dict:
        start_index = int(request_dict['ExclusiveStartKey']['RangeKeyElement']['S']['S'][-1]) + 1
      else:
        start_index = 0

      count = min(max_index - start_index, limit)
      items = []
      for i in xrange(start_index, start_index + count):
        items.append({'ei': {'S': 'e0'},
                      'sk': {'S': 'p%d' % i}})

      response_dict = {'Count': count,
                       'ConsumedCapacityUnits': 0.5}
      if not is_count:
        response_dict['Items'] = items

      if start_index + count < max_index:
       response_dict['LastEvaluatedKey'] = {'HashKeyElement': {'S': items[-1]['ei']},
                                            'RangeKeyElement': {'S': items[-1]['sk']}}

      return httpclient.HTTPResponse(request, 200,
                                     headers={'Content-Type': 'application/json'},
                                     buffer=StringIO(json.dumps(response_dict)))

    # Get session token from Amazon (no need to mock that).
    client = dynamodb_client.DynamoDBClient(schema=vf_schema.SCHEMA)
    self._RunAsync(client.GetItem, vf_schema.TEST_RENAME, DBKey('1', 1), attributes=None, must_exist=False)

    with mock.patch('tornado.httpclient.AsyncHTTPClient', MockAsyncHTTPClient()) as mock_client:
      mock_client.map(r'https://dynamodb.us-east-1.amazonaws.com', partial(_MakeResponse, 5))

      # Limit = None.
      posts = self._RunAsync(Post.RangeQuery, client, 'e0', None, None, None)
      self.assertEqual(len(posts), 2)

      # Limit = 2.
      posts = self._RunAsync(Post.RangeQuery, client, 'e0', None, 2, None)
      self.assertEqual(len(posts), 2)

      # Limit = 5.
      posts = self._RunAsync(Post.RangeQuery, client, 'e0', None, 5, None)
      self.assertEqual(len(posts), 5)

      # Limit = 7.
      posts = self._RunAsync(Post.RangeQuery, client, 'e0', None, 7, None)
      self.assertEqual(len(posts), 5)

      # Limit = None, count = True.
      count = self._RunAsync(Post.RangeQuery, client, 'e0', None, None, None, count=True)
      self.assertEqual(count, 2)

      # Limit = 2, count = True.
      count = self._RunAsync(Post.RangeQuery, client, 'e0', None, 2, None, count=True)
      self.assertEqual(count, 2)

      # Limit = 5, count = True.
      count = self._RunAsync(Post.RangeQuery, client, 'e0', None, 5, None, count=True)
      self.assertEqual(count, 5)

      # Limit = 7, count = True.
      count = self._RunAsync(Post.RangeQuery, client, 'e0', None, 7, None, count=True)
      self.assertEqual(count, 5)

  def testBatchQuery(self):
    """Test DBObject.BatchQuery."""
    # Create some data to query.
    keys = []
    for i in xrange(3):
      photo_id = Photo.ConstructPhotoId(time.time(), self._mobile_dev.device_id, 1)
      episode_id = Episode.ConstructEpisodeId(time.time(), self._mobile_dev.device_id, 1)
      ph_dict = {'photo_id': photo_id,
                 'user_id': self._user.user_id,
                 'episode_id': episode_id}
      self._RunAsync(Photo.CreateNew, self._client, **ph_dict)
      keys.append(DBKey(photo_id, None))

    # Add a key that will not be found.
    keys.append(DBKey('unk-photo', None))

    photos = self._RunAsync(Photo.BatchQuery, self._client, keys, None, must_exist=False)
    self.assertEqual(len(photos), 4)
    for i in xrange(3):
      self.assertEqual(photos[i].GetKey(), keys[i])
    self.assertIsNone(photos[3])

redpajama_set_name: RedPajamaGithub


Product performance is improved significantly with the newest high-velocity update of ConceptDraw PRO v11. New release increases drawing speeds over 300%.
November 7, 2017, San Jose, California —	CS Odessa introduces a new version of its well-known business graphics and diagramming tool, ConceptDraw PRO v11. Drawing speeds and product performance are dramatically improved with the newest update of ConceptDraw PRO v11.
ConceptDraw PRO is well-known for its ability to exchange documents with Microsoft Visio — the de facto standard in software engineering graphics documents. It is supported by the powerful business solutions located in the Solution Park. It delivers solutions for Project Management, Collaboration, Business Productivity and Diagramming. The variety of solutions available in the Solution Park is constantly expanding to provide professionals ultimate flexibility in their diagramming platform.
ConceptDraw PRO is compatible with Apple macOS and Microsoft Windows and retails for US$199. It is now included in ConceptDraw Office v4 which retails for US$499.


SUNY Oswego communication studies faculty member Dr. David Moody has received a national award for his work on African-American visual popular culture.
Moody, who has taught since 2010 in the broadcasting and mass communication program, earned the Harry Shaw Award in April for outstanding contributions to the field of African-American popular-culture research at the annual conference of the Popular Culture Association/American Culture Association in Chicago.
In 2012, Moody published Political Melodies in the Pews? The Voice of the Black Christian Rapper in the Twenty-first Century Church, and is nearing publication of a book on black identity in film and television. His Ph.D. from Bowling Green State University was in American culture studies with emphasis in critical studies in film, media and culture.


Our entire staff is assembled for one purpose: to serve our patients. Our goal is to provide you with the best possible hearing care we can, based on your individual needs. We provide a comprehensive array of services related to evaluation, rehabilitation and prevention of hearing impairment.
Attuned to the latest advances and products, the staff of Westech Hearing ensures we provide our patients with state of the art technology. Additionally, every product we sell includes the highest level of customer service from our experienced, trusted team.


text:
Sansasyon De Ferrier 1, 2, 3, 4, 5 Group
Flag of Haiti
Trou-du-Nord, Nord-Est, Haiti / Food
Sansasyon De Ferrier 1, 2, 3, 4, 5 Group's loan finished fundraising,
A loan helped to purchase food products.
Sansasyon De Ferrier 1, 2, 3, 4, 5 Group's story
Jaqueline is the organizer in her group, Sansasyon de Ferrier. She resides in the CAP-H region of Haiti, where electricity is rare and water access quite limited. She has four children. Jacqueline manages her own grocery store. She would like to use this loan to invest in several products. Other members of Sansasyon de Ferrier need their loans for such businesses as the retail of food products, coal, and cosmetics. Jacqueline says that her main challenge is the lack of regular customers due to unemployment. She says that her dream is to grow her business to become a major retailer.


text:
Герб Естрикланда () — символ исторической провинции (ландскапа) Естрикланд, Швеция. Также употребляется как элемент официального символа современного административно-территориального образования лена Евлеборг.

История
Герб ландскапа известный по описанию похорон короля Густава Вазы 1560 года.

Описание (блазон)
В усеянном синими шарами серебряном поле червленый лось с золотыми рогами и копытами.

Содержание
Герб ландскапа может увенчиваться герцогской короной.

См. также
 Естрикланд
 Провинции Швеции
 Геральдика Швеции

Источник
 Nevéus C. Ny svensk vapenbok. — Stockholm: Streiffert, 1992. — S. 20, 21.

Гербы ландскапов Швеции
Гербы с изображением лося

redpajama_set_name: RedPajamaWikipedia


Well, today's been an interesting day. We drove down to the dealership and started looking at cars again. Unfortunately some of the ones we'd read about on the dealer's website were either already sold or at one of their other locations. Our salesrep1)Hey, Tyler! worked with us for about 5 hours to help us find a car we both liked and could afford. After all that work, we ended up with the 2013 Nissan Rogue you see here. It's newer than our Tucson was, has a smoother ride and even more head room. While it doesn't have all the advanced features of the Tucson; it was a bit less expensive. This allowed us to include the cost of adding a backup camera2)They'll actually be replacing the Rogue's entertainment console to swap it out with one that has a screen for the backup camera.
2. ↑ They'll actually be replacing the Rogue's entertainment console to swap it out with one that has a screen for the backup camera.


text:
Q: sorting positive and negative integers through two integer arrays We gave the following string:
int [] array = {12, 23, -22, 0, 43, 545, -4, -55, 43, 12, 0, -999, -87}.

There must be two rows, one for storage and the other positive elements for the negative elements of string array, and extracting the necessary logic that will perform the appropriate elements and placing them in the appropriate thread.
In other words, in the line array that is given is to be obtained all the positive elements and be placed in a separate row. Also, all the elements to be obtained and the negative to be placed in a separate row.
You also need to determine the number of duplicates in the string array.
Of course, it is necessary functionality written to be applicable to any number of integers.  But MY teacher said that my code doesn't have a target row and He gave me  an example: Target strings are two additional rows you will place isolated positive and negative values. For example, if you have a string:
int arr = {1,2,3,4, -1, -2, -3, -4}

then the target ranges will be:
int pos = {1,2,3,4}
int hc = {-1, -2, -3, -4}

of course, this should make it programmable and not hard coded, as in this example.   Now how can I improve my code?
public static void main(String[] args) {

    int array1[]= {12, 23, -22, 0, 43, 545, -4, -55, 43, 12, 0, -999, -87};

    System.out.println("Array 1 :");

    Arrays.sort(array1);

    for (int positive: array1) {

        if (positive >= -1)
            System.out.println("Positive numbers :" + positive+ "\t");
        }
        System.out.println();
        System.out.println("Array 2 :");

        for (int negative: array1) {
            if (negative >= -1) {

            }else{ System.out.println("Negative numbers :" +negative);
            }

        }
        System.out.println();

        for (int i = 0; i < array1.length -1; i++) {
             if (array1[i + 1 ] == array1[i]) {
                 System.out.println("Duplicate element found :" + array1[i]);
                 i = i + 1;

             }

        }

    }
}

A: If i have understood your question correctly, you want to make new arrays containing the positive and negative numbers,
Using your variable names i would go for something like this solution:
public static void main(String[] args) {

    // Declare variables
    int[] array1 = {12, 23, -22, 0, 43, 545, -4, -55, 43, 12, 0, -999, -87}, pos, hc;
    int positive = 0, negative = 0;

    // Check how many positive and/or negative numbers
    for (int i : array1)
    {
        if (i >= 0)
        {
            positive++;
        } else
        {
            negative++;
        }
    }

    // Make exact size arrays
    pos = new int[positive];
    hc = new int[negative];

    // Reset variables for new purpose
    positive = 0;
    negative = 0;

    //Put numbers in correct array
    for (int i : array1)
    {
        if (i >= 0)
        {
            pos[positive] = i;
            positive++;
        } else
        {
            hc[negative] = i;
            negative++;
        }
    }

    // Display arrays
    System.out.print("Starter array: ");
    for (int i: array1)
    {
        System.out.print(" " + i);
    }

    System.out.print("\nPositive array: ");
    for (int i: pos)
    {
        System.out.print(" " + i);
    }

    System.out.print("\nNegative array: ");
    for (int i: hc)
    {
        System.out.print(" " + i);
    }

}

This outputs:
Starter array:  12 23 -22 0 43 545 -4 -55 43 12 0 -999 -87
Positive array:  12 23 0 43 545 43 12 0
Negative array:  -22 -4 -55 -999 -87

A: try
 int array1[]= {12, 23, -22, 0, 43, 545, -4, -55, 43, 12, 0, -999, -87};

 System.out.println("Array 1 :");

 Arrays.sort(array1);
 ArrayList<Integer> pos = new ArrayList<Integer>();
 ArrayList<Integer> neg = new ArrayList<Integer>();
 for (int num: array1){
  if (num>= 0)
       pos.add(num);
   else
       neg.add(num);
}
 System.out.println();

 if(pos.size()>0)
 {
 int[] positive = new int[pos.size()];
 positive = pos.toArray(positive);
 pos=null;
 for (int num: positive)
      System.out.println("Positive numbers :" + num+ "\t");
 }

 if(neg.size()>0)
 {
 int[] negative = new int[neg.size()];
 negative = pos.toArray(negative);
 neg=null;
 for (int num: negative)
      System.out.println("Negative numbers :" + num+ "\t");
 }

for (int i = 0; i < array1.length -1; i++) {
    if (array1[i + 1 ] == array1[i]) {
        System.out.println("Duplicate element found :" + array1[i]);
        i = i + 1;

        }

    }

A:    sepratePositiveNegative(int[] arr) {
        int size  = arr.length;
        int k =0;
        for(int i =0;i <size; i++){
            int temp = 0;
            if(arr[i]<0) {
                temp = arr[i];
                arr[i] = arr[k];
                arr[k] = temp;
                k++;
                System.out.println(arr[i]);
            }
        }

redpajama_set_name: RedPajamaStackExchange


Did you know that when we sleep, we go through 5 different stages? The experience differs with each individual stage. Knowing these stages will help you maximize the energy you gain from your daily dose of sleep or naps.
In the first stage of sleep, we all have consciously experience it before. Try to recall the times when we fell asleep during long hours of lectures, or when your mind wanders off and you find yourself day-dreaming. It really feels good being in this stage, our mind and body are in the state of relaxation. This stage is merely the doorway to our sleep.
During the second stage of sleep, our mind is trying to shut itself down. At this point, the slightest disturbance in our environment would wake us. Once awaken from this stage of sleep, you'll swear that you've been awake all this time, when in fact you've actually fallen asleep.
Once we're in the third and fourth stages of sleep, we can officially declare that we are truly asleep. These stages are called deep sleep. During deep sleep, the activity of our mind and physical body are at the lowest point of the day. Our muscles and organs are nourished and replenished during this stage. The lack of these stages would cause us to feel tired once we've awaken from our sleep.
The fifth stage of sleep is called Rapid Eye Movement, or simply REM sleep. As the name suggests, our eyes move rapidly during this stage. The dreams we've experience during our sleep occurs at this stage.
Understanding these stages in our sleep helps us to gain more quality sleep.
Jimmy Law writes on a wide range of topics. Some of his favorite subjects include teething and vomiting and baby teething symptoms.