text:
Das Springpferd Goldfever ist ein 1991 geborener Fuchshengst, vorgestellt wurde er von Ludger Beerbaum. Er stammt von dem Zangersheider Hengst Grosso Z aus einer Mutter von Galvano ab und trägt selbst den Brand des Hannoveraner-Zuchtverbandes. 2009 wurde er im Rahmen des CHIO Aachen, wo er 2002 und 2003 den Großen Preis gewann, aus dem Sport verabschiedet. Mit einer Gewinnsumme von rund 2,8 Mio. Euro ist er eines der erfolgreichsten Springpferde aller Zeiten. Daneben ist er auch ein gekörter und leistungsgeprüfter Zuchthengst. Nachdem er zwischen 2001 und 2009 nur im Sport eingesetzt wurde, steht er nach seiner Verabschiedung in Aachen wieder als Zuchthengst zur Verfügung. Seine herausragenden Vererberqualitäten sieht man an seiner Tochter Gotha, die international erfolgreich mit Ludger Beerbaum unterwegs ist.

Dopingvorwürfe 2004
Während der Olympischen Spiele 2004 in Athen wurde Goldfever positiv auf die verbotene Substanz Betamethason getestet. Ludger Beerbaum verteidigte sich vehement gegen die erhobenen Dopingvorwürfe und gab an, dass die Substanz durch eine Salbe, die zur Behandlung einer kleinen Verletzung aufgetragen wurde, in den Blutkreislauf des Pferdes gelangt war. Er übernahm die Verantwortung dafür, legte aber Wert auf die Feststellung, dass es sich nicht um bewusstes Doping zur Leistungssteigerung gehandelt habe. Im September 2005 wurde die Disqualifikation des Paars Beerbaum/Goldfever vom CAS endgültig bestätigt. Beerbaum verlor seine Goldmedaille, ebenso wie die anderen deutschen Reiter, die stattdessen die Bronzemedaille erhielten.

Erfolge
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Europameisterschaft:

 2007: 3. Platz EM in Mannheim im Einzel
 2007: 2. Platz EM in Mannheim mit der Mannschaft

Einzelnachweise

Springpferd
Zuchthengst
Olympiapferd
Pferd (Deutschland)


Approach of the portal and you are faced with a likely adversary. Lit only by flames, this anubic creature regards you with its duties in mind. The dark profile is broken up by its gold markings, with spacing cut into the shapes. Through use of the fatter line godpaint, this sentinel has a seriously strong presence.


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Home > Strategy > Kingdom Under Fire II finally - FINALLY - has a western release window
Kingdom Under Fire II finally - FINALLY - has a western release window
One of my favourite experiences back on the original XBox was a humble title from Korea called Kingdom Under Fire. It was basically everything I loved in video games - it was a blend of real-time strategy, RPG, and Dynasty Warriors-like action, and it really worked as well as the best case scenario you could think up. It was so good that I have kept and Xbox around in the years since specifically so I can pull that game out (and its sequel) and play it from time to time.
A proper sequel to Kingdom Under Fire has been in development for a very, very long time. Kingdom Under Fire II was first announced over a decade ago, back in 2008. Since then it has gone through all kinds of iterations and half-announcements, but there is finally solid proof that it is really happening: publisher Gameforge has picked it up for localisation, has promised a 2019 release window, and has released a spiffy new trailer.
Currently the game is only slated for a PC release, but in years past some of those half-promises have included a PlayStation 4 release, so the ongoing saga around Kingdom Under Fire II looks set to continue for some time. The main thing is that it's finally getting a release. I can't wait.
Please help keep DDNet running:

redpajama_set_name: RedPajamaCommonCrawl


text:
\section{INTRODUCTION}
\label{intro.sec}

ELM WDs or pre$-$ELM WDs are helium core white dwarfs
with mass below
0.30$M_{\odot}$ \citep[][]{2019ApJ...871..148L}.
Given their extreme low mass and the current age of our Universe,
they can only be formed within close binary systems.
The progenitor of the ELM WD are  thought
to be a low mass star with mass between 1.0$M_{\odot}$ and 1.5$M_{\odot}$, being stripped off its hydrogen envelope
by its companion  either through the stable Roche lobe overflow channel (RL channel) or the common envelope ejection channel (CE channel) \citep[][]{2002MNRAS.336..449H, 2017MNRAS.467.1874C, 2018ApJ...858...14S, 2019ApJ...871..148L}.
ELM WDs with mass lower than 0.18$M_{\odot}$ are thought to be  produced only in RL channel, since in the CE channel, the thick envelope can't be thrown off and the two star will  merge when
the mass of the helium core is lower than 0.21$M_{\odot}$\citep[][]{2018ApJ...858...14S, 2019ApJ...871..148L}.
The pre-ELM phase happened at the end of the mass transfer of the RL channel, where the donor may still bear a thick
bloated  hydrogen envelope
sustained by  hydrogen burning for  up to Gyrs before they contract  to white dwarf cooling track\citep[][]{2014A&A...571A..45I}.
Those bloated pre-ELMs have similar color as main-sequence A and F star and hard to be distinguished by color or low resolution spectra\citep[][]{2018MNRAS..475.2480,2021MNRAS.505.2051E}. The mass of ELM WD formed in the RL channel lies between  0.14 and 0.4 $M_{\odot}$. The minimum mass is set by the bifurcation initial period\citep[][]{1998A&A..191.57,2019ApJ...871..148L}, below which the donor cannot develop a compact core and evolve to a brown dwarf likely \cite[][]{2004ApJ...616.1124N,2017MNRAS.467.1874C}.
Different evolution calculation\citep[e.g.][]{2016A&A...595...35,2018MNRAS..475.2480,2019ApJ...871..148L}  show that the lower limit of ELM WD is around 0.14-0.16 $M_{\odot}$.  The observational mass limit seems to coincident with the theoretical result \citep[e.g.][]{2016ApJ...818..155B}. \citet{2021MNRAS.508.4106E} listed  the 21 spectral confirmed pre-ELM WD systems, 6 have masses lower than 0.14 $M_{\odot}$,
but still consistent with the theoretic estimation considering their uncertainties.

In this work we report a very low mass pre-ELM WD, ID70904216, discovered in LAMOST low resolution spectral survey. With the help of LAMOST radial velocity curve, GAIA Dr3 \citep[]{2021Gaia} distance and ZTF\citep[][]{2019pasp..131.018002} multi-color light curves, the  mass of ID70904216 could be  constrained to $0.08^{+0.06}_{-0.03}  M_{\odot}$, which is lower than any known ELM WD.
Testing the lower limit of ELM WD is important  for studying the theories of mass transferring (MT) and accreting process,
the  Common Envelope phenomena (CE),
angular momentum loss (AML) due to magnetic braking and Gravitational wave radiation, radiation driven evaporation,
and many other physical mechanisms related to close binary evolution
\citep[][]{1986ApJ...311..742I, 2014A&A...571A..45I, 2017MNRAS.467.1874C, 2018ApJ...858...14S, 2019ApJ...871..148L}.

This paper is organized as follows.
In Section \ref{sec.obs} the existing data and new observations are gathered and described.
In Section \ref{sec.results} the data analyzing results are illustrated.
The summaries and discussions are shown in Section \ref{sec.sum}.

\section{Observations}
\label{sec.obs}

In this Section,
both archival and newly acquired observational data for ID70904216
are present.
For convenience through out this work,
we name the visible star as star 1, the primary,
and the invisible star as star 2, the secondary.
Phase 0 represents the moment when the visible star is at the superior conjunction point.

\subsection{Spectroscopic observation}
\label{sec:spectra}

ID70904216 was first discovered as a candidate of binaries with
compact object in LAMOST low resolution(R $\approx$ 1800) survey\citep{2012RAA....12.1197C,2012RAA....12..723Z}.
In regular data release, the spectra of sub-exposures are  combined  to remove cosmic rays.  To take full advantage of LAMOST spectra in time domain,
the sub-exposure spectra as well as RV measurement of individual spectrum were released in 2021 \citep[][]{2021RAA....21..249B}.
ID70904216 has 8 individual low resolution spectra
in 3 nights from 2016 to 2021,
as listed in Table \ref{tab.sp_obs}. The LAMOST spectra show a RV variation
of more than 560km/s, indicating the system should be a close binary with possible  compact companion.

Two additional low resolution spectra were acquired
in  the Double Spectrograph (DBSP) of
the 200 inch  Hale telescope at Palomar Observatory(P200) via the TAP (Telescope Access Program for China based astronomers) \footnote{http://info.bao.ac.cn/tap/} project.
The dichroic filter was set to $D\-55$.
For the blue side,
the grating was set to 1200 lines/mm, 5000\AA\  blaze,
and the angle was set to $35^\circ52^\prime$
(center wavelength: 4500\AA).
For the red side,
the grating was set to 1200 lines/mm, 7100 $\AA$ blaze,
and the angle was set to $42^\circ02^\prime$
(center wavelength: 6600\AA).
The slit width was set to $1.5^{\prime\prime}$,
according to the seeing.
The spectra cover wavelength from 3900 to 5250\AA\ in the blue,
and from 5800 to 7400\AA\  in the red,
with a resolution  $R$  $\approx2100$ and $\approx3200$, for the blue and red respectively.
The IRAF package is used to handle raw data processing,
including bias and flat correction, cosmic ray removal,
spectral extraction and wavelength calibration.
The same method as in  \cite{2021RAA....21..249B} was applied to
measure the RV of P200 spectra.
Observation information as well the measured spectral parameters are shown in Table \ref{tab.sp_obs}.

\begin{table*}
\caption{Spectroscopic observations and estimated parameters of ID70904216.
Note the DATE column represents the time zone observation night,
and the HJD represents the heliocentric time at the middle of exposure.
The signal to noise ratios (SNR) for single exposures are between 10 and 20, the typical errors in this SNR range are 150k, 0.25dex and 0.15dex for $T_{\rm eff}$, log $g$ and [Fe/H], respectively.
\label{tab.sp_obs}}
\setlength{\tabcolsep}{5.0pt}
\begin{center}
\begin{tabular}{cccccccccc}
\hline\noalign{\smallskip}
DATE & HJD & RV  & Phase & RVCorr & $T_{\rm eff}$ & log $g$ & [Fe/H] & EXPTIME & Tel.$/$Ins. \\
     & day & km/s  &     & km/s   & K             & dex     & dex    & s & \\
\hline\noalign{\smallskip}
20161128 & 2457720.9407 &  141.98$\pm$4.49  & 0.62 &  145.16 & 7347 & 4.14 &  0.11 &1800 & LAMOST$/$LRS \\
20161128 & 2457720.9636 &  236.38$\pm$4.86  & 0.72 &  240.97 & 7357 & 4.08 &  0.15 &1800 & LAMOST$/$LRS \\
20161128 & 2457720.9872 &  209.65$\pm$4.42  & 0.83 &  213.84 & 7323 & 4.05 &  0.14 &1800 & LAMOST$/$LRS \\
20171120 & 2458077.9763 & -132.78$\pm$7.92  & 0.04 & -133.71 & 7334 & 4.25 & -0.11 &1800 & LAMOST$/$LRS \\
20171120 & 2458077.9992 & -303.82$\pm$6.74  & 0.14 & -307.30 & 7608 & 4.37 & -0.06 &1800 & LAMOST$/$LRS \\
20171120 & 2458078.0228 & -374.01$\pm$10.12 & 0.25 & -378.54 & 7478 & 4.36 &  0.11 &1800 & LAMOST$/$LRS \\
20210603 & 2459368.9314 & -337.18$\pm$3.34  & 0.15 & -338.94 & 7525 & 4.14 &  0.06 &1200 &  P200$/$DBSP \\
20210603 & 2459368.9787 & -299.28$\pm$4.09  & 0.37 & -300.79 & 7197 & 4.07 &  0.01 &1200 &  P200$/$DBSP \\
20211010 & 2459498.0289 & 148.55$\pm$7.30   & 0.87 &  151.83 & 7401 & 4.11 &  0.09 &1800 & LAMOST$/$LRS \\
20211010 & 2459498.0512 & -24.90$\pm$7.89   & 0.98 &  -24.21 & 7099 & 3.94 &  0.25 &1800 & LAMOST$/$LRS \\
\noalign{\smallskip}\hline
\end{tabular}
\end{center}
\smallskip
\end{table*}

\begin{figure*}[htbp!]
\center
\includegraphics[width=0.98\textwidth]{ID7090sexp_hb.eps}
\includegraphics[width=0.98\textwidth]{ID7090combfit.eps}
\includegraphics[width=0.98\textwidth]{ID7090combfit_res.eps}
\caption{
The upper panel: the single exposure spectra of ID70904216 from
LAMOST and P200.
The spectra from bottom to top are in phase ascending order,
and adjacent spectra are shift by 0.5 in y direction to make a clear view.
The phases are shown in the right side.
Details are shown in Table \ref{tab.sp_obs}.
The middle panel:
The combined spectrum of the blue band (blue),
over-plotted with its best fitting template (red).
The lower panel:
The residual in the fitting of combined spectrum of the blue band.
}
\label{spfig}
\end{figure*}

\subsection{Light Curves}
\label{sec:lightcurve}

ID70904216 was firstly observed by the Catalina survey
between 2007 and 2012,
and classified as ellipsoidal variable
with a period of 0.2196580 days and an amplitude of 0.24mag
\citep{2014ApJS..213....9D}.
Between 2012 and 2018,
ASAS-SN sparsely observed this target in V band for more than a few hundred times,
but no classification is available since it is too faint.
\citep[][]{2019MNRAS.486.1907J}.
The ATLAS survey (Asteroid Terrestrial-impact Last Alert System),
operated since 2015 using cyan and orange filters,
classified this target as \textbf{NSINE},
indicating sinusoidal variables with large residual noise
\citep{2018AJ....156..241H}.
The ZTF survey,
operated since 2018 using g, r and i bands,
classified this target as EW,
with a period of 0.219655 days in g band and 0.2196582 days in r band
\citep[][]{2020ApJS..249...18C}.
Combing the Catalina and ZTF data spanning 14 years, we derive a period of 0.219658±0.000002 days.
The adopted ephemeris of the system is,
\begin{equation}
T (\phi = 0) = 2454000.0198(5)HJD + 0.219658(2) \times N,
\end{equation}
where $\phi =$  0 corresponds to the visible star in superior conjunction,
and $HJD$ is the heliocentric Julian Date.
While the period estimation well matches the data
from Catalina, ASAS$\-$SN and RV data(see Section \ref{sec:orbit}),
the zero point has relatively larger uncertainties,
since the value is obtained from spare sampling,
instead of continuous high time resolution monitoring.

 \begin{figure}[htbp!]
\center
\includegraphics[width=0.48\textwidth]{lc.eps}
\caption{Folded RV curves and LCs in different bands
($V$ band of Catalina,
$g$, $r$ and $i$ bandS of ZTF)
with a period of 0.2196580 day.
The phases of
superior conjunction ($\phi$ = 0 or 1),
quadrature ($\phi =$ 0.25 and 0.75),
and inferior conjunction  $\phi =$ 0.5
are marked with vertical gray lines.
A calculated RV curve is shown
using best fit K1$=317.33km/s$ and V$_{sys}=-70.31km/s$.
}
\label{show.fig}
\end{figure}

\subsection{Multi-band photometry}
\label{sec:photometry}

According to the GALEX Search Tool \footnote{http://galex.stsci.edu/GR6/?page=mastform},
ID70904216 has two records in GALEX archive\citep{2017ApJS..230...24B},
 $OBJID=$ $6376439803911605972$ and $6376439771699347883$.
For both records, only $NUV$ band measurements are valid,
which are $20.66\pm0.16$ and $20.24\pm0.15$, in magnitude, respectively.
Via CasJob \footnote{http://galex.stsci.edu/casjobs/},
a joint query between $VisitPhotoObjAll$, $VisitPhotoExtract$ and $visitImg$
shows that the target was visited 4 times (see Table \ref{tab.galex}.
The latest two visits merge into the combined record of $OBJID=6376439803911605972$,
while the two in 2004 merge into the combined record of $OBJID=6376439771699347883$.
One of the four visits has reported a FUV calibrated flux using NUV position,
$3.989049\pm4.171614 micro Jy$ ($22.39783\pm1.135702$ in mag), though there is little signal in the combined image by visual inspection.
This value has apparently large error, thus could be the upper limit of FUV flux.

\begin{table}
\caption{The GALEX observation of ID70904216. Only NUV measurements are available.
\label{tab.galex}}
\setlength{\tabcolsep}{4.5pt}
\begin{center}
 \begin{tabular}{cccc}
\hline\noalign{\smallskip}
DATE & JD(day) & NUV mag & PHASE \\
\hline\noalign{\smallskip}
20070908 & 2454351.9646 & 20.89$\pm$0.27 & 0.24 \\
20061012 & 2454021.1541 & 20.46$\pm$0.20 & 0.22 \\
20040810 & 2453231.9007 & 20.29$\pm$0.20 & 0.11 \\
20040810 & 2453231.9692 & 20.13$\pm$0.21 & 0.42 \\
\noalign{\smallskip}\hline
\end{tabular}
\end{center}
\smallskip
\end{table}

No X-ray catalogues match ID70904216 directly according to \textbf{CDS Portal}
\footnote{http://cdsportal.u-strasbg.fr//}.
The upper limit is checked via the HIgh-energy LIght-curve GeneraTor
\footnote{http://xmmuls.esac.esa.int/upperlimitserver/}.
The \textbf{XML-NEWTON SLEW} mission provides upper limits
in the $0.2-2$, $2-12$ and $0.2-12$ flux bands
(7.1073e-13, 5.7056e-12 and 1.4153e-12 $erg/s/cm^2$ respectively, on May 16, 2009).
The \textbf{ROSAT-SURVEY} provides an upper limit of 3.5579e-13 $erg/s/cm^2$
in $0.2-2$ flux bands on Nov. 17, 1990.
The \textbf{INTEGRAL} mission provides upper limits
in the $20-40$, $40-60$ and $60-100$ flux bands
(1.0381e-11, 8.9913e-12 and 9.4841e-12 $erg/s/cm^2$ respectively, on Nov. 7 2003).
The upper limit of X-ray to optical flux ratio
$\log(f_X/f_V)$ can be estimated as $\approx-0.24$,
which is within the chromosphere active range
\citep[][]{2019RAA....19...98H}.

In the near infrared band,
ID70904216 was visited
by the Two Micron All Sky Survey on Sep. 29 1998 \citep[][]{2006AJ....131.1163S},
corresponding to a phase of 0.097,
with mag J $=16.754\pm0.134$,
mag H $=16.221$ and mag K $=15.941$.
However the related $Qflg$ is $BUU$ and $Rflag$ is $200$,
indicating no source is detected in H and K band
and the upper limit is adopted.
Similarly in the WISE observations,
the $qph$ flat is $ACUU$, indicating
only the $W1$ band is reliable.
Fortunately the VISTA Hemisphere Survey (VHS) \citep[][]{2013Msngr.154...35M}
 provide better Y, J, H and Ks magnitudes.
All their bit wise processing warning/error flags are 0,
indicating reliable measurements.
So we discard the unreliable photometry, leave VISTA and WISE W1 for the following analysis.
The multi-band photometry measurements are collected in Table \ref{tab.mags}.

\begin{table*}
\caption{Multi-band photometry measurements for ID70904216. \label{tab.mags}}
\setlength{\tabcolsep}{4.5pt}
\begin{center}
\begin{threeparttable}
\begin{tabular}{cccc}
\hline\noalign{\smallskip}
Filter & Magnitude & Reference \\
\hline\noalign{\smallskip}
GALEX NUV & 20.6582$\pm$0.1643\tnote{1} & \citet[][]{2017ApJS..230...24B} \\
SDSS u & 18.441$\pm$0.018 & \citet[][]{2020ApJS..249....3A} \\
SDSS g & 17.350$\pm$0.005 & \citet[][]{2020ApJS..249....3A} \\
SDSS r & 17.186$\pm$0.006 & \citet[][]{2020ApJS..249....3A} \\
SDSS i & 17.195$\pm$0.006 & \citet[][]{2020ApJS..249....3A} \\
SDSS z & 17.280$\pm$0.014 & \citet[][]{2020ApJS..249....3A} \\
PS1 g & 17.3403$\pm$0.0529 & \citet[][]{2016arXiv161205560C} \\
PS1 r & 17.2061$\pm$0.0059 & \citet[][]{2016arXiv161205560C} \\
PS1 i & 17.2487$\pm$0.0133 & \citet[][]{2016arXiv161205560C} \\
PS1 z & 17.2694$\pm$0.0162 & \citet[][]{2016arXiv161205560C} \\
PS1 y & 17.3129$\pm$0.0222 & \citet[][]{2016arXiv161205560C} \\
GaiaEDR3 G  & 17.1381$\pm$0.0073 & \citet[]{2021Gaia} \\
GaiaEDR3 BP & 17.2973$\pm$0.0240 & \citet[]{2021Gaia} \\
GaiaEDR3 RP & 16.8414$\pm$0.0206 & \citet[]{2021Gaia} \\
2MASS J	& 16.754$\pm$0.134 & \citet[][]{2003cvs..book.....W} \\
2MASS H & 16.221\tnote{2} & \citet[][]{2003cvs..book.....W} \\
2MASS Ks & 15.941\tnote{2} & \citet[][]{2003cvs..book.....W} \\
WISE W1 & 16.428$\pm$0.079 & \citet[][]{2014yCat.2328....0C} \\
WISE W2 & 16.998$\pm$0.457\tnote{3} & \citet[][]{2014yCat.2328....0C} \\
WISE W3 & 12.302\tnote{3} & \citet[][]{2014yCat.2328....0C} \\
WISE W4 & 8.722\tnote{3} & \citet[][]{2014yCat.2328....0C} \\
VISTA Y  & 16.7193$\pm$0.0131 & \citet[][]{2013Msngr.154...35M} \\
VISTA J  & 16.6129$\pm$0.0146 & \citet[][]{2013Msngr.154...35M} \\
VISTA H  & 16.5509$\pm$0.0164 & \citet[][]{2013Msngr.154...35M} \\
VISTA Ks & 16.4528$\pm$0.0393 & \citet[][]{2013Msngr.154...35M}  \\
\noalign{\smallskip}\hline
\end{tabular}
\begin{tablenotes}
\footnotesize
\item[1] This is the combined magnitude for $OBJID=$ $6376439803911605972$.
\item[2] This is an upper limit.
\item[3] The photometry quality flag is not good and no error is provided for W3 and W4.
\end{tablenotes}
\end{threeparttable}
\end{center}
\end{table*}

\subsection{Distance, Kinematics and Extinction}
\label{sec:distance}

In Gaia EDR3 \citep[]{2021Gaia},
ID70904216 is $source\_id=2652639593773429120$.
Its parallax is $0.69426mas$ and parallax error is $0.085375mas$.
The $RUWE$ is $1.0642716$,
implying no significant excess noise
and no indicative of parallax estimation problem.
The parallax bias, according to \citet[][]{2021A&A...649A...4L},
is $-0.031682mas$, yielding to a corrected parallax of $0.72594$,
and corresponding to distance of $1377.5^{+183.6}_{-145.0}pc$,
and distance modulus of $10.695^{+0.241}_{-0.272}$.
The distance using Bayes technology,
according to \citet[][]{2021AJ....161..147B},
is $1340.4^{+185.7}_{-132.3}pc$.
In case the effective temperature is unchanged,
a smaller distance indicates smaller stellar radius and mass estimation.
Here we choose to use the distance of $1377.5^{+183.6}_{-145.0}pc$
in our following work.

ID70904216 is within the southern Galactic cap,
and is $1054pc$ below the Galactic plane according to its distance.
Its proper motion in Gaia EDR3 is $pmra=-0.2656mas$ and $pmdec=0.6671mas$.
Together with system velocity of $-70.31km/s$ from our orbit fitting(see  Section\ref{sec:orbit}),
the 3D motion in LSR $(U,V,W)_{LSR}$ $=$ $(9.94km/s, -27.93kms, 60.325kms)$,
indicating a thin disk object
($P_{thin}\approx66\%$, $P_{thick}\approx32\%$)
\citep[][]{2013ApJ...764...78R}.

The 3D dust map of \citet[][]{2019ApJ...887...93G},
which is based on Gaia parallaxes and stellar photometry
from Pan-STARRS1 and 2MASS,
gives an extinction coefficient $\alpha$ of 0.07.
Actually the coefficient $\alpha$ reaches 0.07 at $DM=6.25$ and remains unchanged for larger $DM$s.
The corresponding extinction coefficient $E(B-V)$ is $0.062$ or $0.069$,
according to the two transformation formula of \citet[][]{2019ApJ...887...93G}.
 2D extinction  based on  IRAS and COBE/DIRBE data show lower value,
 $E(B-V)$ from \citet[][]{1998ApJ...500..525S}  and  \citet[][]{2011ApJ..737103}  are  0.0506$\pm$0.0006 and  0.0435 $\pm$ 0.0005 respectively. Since the 2D extinction represent the total extinction  and should be the upper limit in that direction,
 \citet[][]{1998ApJ...500..525S} value of
 $0.05\pm0.001$ is adopted,
and the corresponding extinctions in g, r, i and Gaia G bands are 0.185, 0.136, 0.102 and 0.138, respectively,
based on the extinction law of \citet[][]{1989ApJ...345..245C} and the band effective wavelength (adopted from the WD code for consistency).

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

\subsection{Spectral parameters}
\label{sec:spparam}
The magnitude is relatively faint,
the SNR of both the LAMOST and P200 spectra are between 10 and 20(see Fig\ref{spfig}).
The spectra
are dominated by
plateau Ca II H $\&$ K in absorption,
normal  Balmer series,
weak Mg I triplets and Ca II Triplets,
nearly invisible G band, Ca I 4226 line and  Paschen series,
suggesting our target is an early F-type star.
All of these lines are in absorption.
Helium lines are invisible in all the spectra.
The UlySS package \citep[][]{2009A&A...501.1269K} is used
to match the  low resolution spectra
to the ELODIE high resolution models,
to derive the stellar parameters.
The parameters for each single exposure are listed in Table \ref{tab.sp_obs}.
Since the SNR of each individual spectrum is relatively low,
 all the single exposures were shifted to the rest frame and combined to get a spectrum with higher SNR. The stellar parameters derived from the rest frame co-added spectrum are $T_{\rm eff}=7198\pm150K$,
log $g$=4.29$\pm$0.25dex and [Fe/H]=0.08$\pm$0.15dex
\footnote{As the error given by UlySS package is unrealistically small, the typical measurement error from https://www.lamost.org/dr8/v1.1/doc/release-note are adopted.},
which agrees with with the average of the individual measurement,i.e., $T_{\rm eff}=7361\pm139K$,
log $g$=4.14$\pm$0.13dex and [Fe/H]=0.08$\pm$0.12dex.

The best fit model and the residuals are shown
in the middle and bottom panel of Fig.\ref{spfig}, respectively.
As marked in the figure, there are a few lines that are
slightly deeper than the model in the residual spectrum.
Considering the low resolution and relative low SNR of individual spectra,
it may also be caused by the improper convolution profile within the co-adding and fitting step.
Further high resolution spectroscopic observation will be useful
to verify  the stellar parameters and element abundance,
and then better understand the nature of this binary system.

\subsection{Spectral Energy Distribution fitting}
\label{sec:sedfit}

Since the photometry  varies with the phase
by up to 30\%,
the phase averaged magnitudes should be used with higher priority to obtain a good SED fit. Considering our target is in a close binary system, interaction may change their evolution path, thus  we only fit the SED with spectral template to derive the temperature and radius, rather than fitting with stellar evolution model.

ID70904216 was observed by Pan-STARRS for
14, 22, 20, 15 and 12 times in g, r, i, z and y bands,
respectively.
Nevertheless,
the sampling time are not evenly distributed within the period,
and the epochs for different bands are different.
With model light curves from preliminary fitting and
the real observation phases from PS1 survey,
we calibrate the PS1 magnitude to the average magnitude of the light curve of the corresponding filter.
The corrections
from PS1 magnitudes to phase averaged magnitudes
are -0.048, -0.008, -0.029, -0.018 and -0.010,
for g, r, i, z and y bands, respectively.
GAIA and SDSS g, r, i and z are not used for their similar color to PS1,
SDSS u was observed at phase 0.87, the correction is 0.0023,
which is  much smaller than the magnitude error(0.018).
In the infrared band, we use VISTA data and WISE W1 band.
The Modified Julian Day of the VISTA observation is $55401.2389797$,
corresponding to a phase of $\approx0.37$, at which the magnitude is close to the average value. Thus the corrections are small, i.e., $0.00069$, $0.00167$ and $0.00183$, for J, H and Ks band, respectively.
As we will see that even the correction effect on the PS1 data is very small,
we decide to ignore the VISTA and SDSS u corrections so as to avoid over correction.
In the UV band, GALEY NUV is our only choice.
We have also ignored the corrections for WISE and GALEX bands,
since the target is relatively faint in those bands, observation uncertainties are larger than corrections.

Since the SED fitting is only sensitive to the temperature,
we fixed log $g$=4.40 (from light curve fitting, section\ref{sec:wdfit})
and [Fe/H]$=0.08$ (from spectral estimation).
The log $g$ from light curve fitting is adopted since
the gravitational potential is better described by the shape of the light curve, thus the log $g$ could be better solved than from the low resolution spectrum.
We have tried to alter  log $g$ to 4.15 and  [Fe/H] to 0.0 respectively, the corresponding change of  $T_{\rm eff}$ are $22K$ and $10K$, respectively.
As a result, the effects of both log $g$ and [Fe/H] on $T_{\rm eff}$ are negligible.
The extinction is  fixed to 0.05 according to Section \ref{sec:distance}.
The fitting result,
using corrected PS1 magnitudes, SDSS u, GALEX NUV mag, VISTA J, H, Ks mag, and WISE W1,
is shown in the upper panel of Fig. \ref{fig.sedfit}.
The model parameters are $T_{\rm eff}=7440K$, log $g=4.40$ and [Fe/H]=0.08.

To get a proper temperature range,
The correlation between extinction and temperature are further tested.
As shown in Fig. \ref{fig.sed_teff_ebv}, $T_{\rm eff}$ linearly correlated with $E(B-V)$.
As   $E(B-V)$ increase from 0.04 to 0.07,  $T_{\rm eff}$ rise about 200K.
Different combination of filter sets have  been tested to  evaluate the effect on the temperature determination.
Comparing the blue and green solid, dashed and dotted lines,
one could see that the inclusion of WISE W1 band has little effect, while the GALEX NUV band  lowers the temperature by $\approx 30K$.
Comparing the blue and green lines,
the phase correction on PS1 data   raises the temperature by $\approx 20K$.

To test the flux contribution of the unseen secondary(assuming a white dwarf), we include the
FUV upper limit in the SED fitting, the result is show in the lower pannel of Fig.\ref{fig.sedfit} and  the red lines in Fig.\ref{fig.sed_teff_ebv}. Comparing the green and the red line in Fig.\ref{fig.sed_teff_ebv}, as the WD temperature increase from 12000K to 22000K, $T_{\rm eff}$ of star 1 Drops about 40K.
With the constraint of FUV flux, the companion WD could be limited to  cooler than 22000K, and the contribution from the hot component in the optical bands
are on the order of 1\%.

Assuming the $T_{\rm eff} \sim$ 7440K and  distance of $1377.5kpc$,
the radius of star 1 can be estimated to be $\approx0.283R_{\odot}$,
Alternatively,
the radius can also be estimated using Gaia G band magnitude for comparison.
As discussed in Section \ref{sec:distance},
ID70904216 has
Gaia g $=17.1381$,
parallax $0.72595mas$,
and Gaia g band extinction $\approx0.13$ based on $E(B-V)\approx0.05$.
The absolute Gaia g band magnitude is estimated to be $\approx6.31$.
Using Bolometric Correction on Gaia g band $BC_G=0.07$
\citep[][]{2018gaia},
the bolometric magnitude $M_{bol}$ is $\approx6.38$.
If the effective temperature is $T_{\rm eff}\sim 7400\pm100K$,
the radius can be estimated to be $R_1=0.28\pm0.01R_{\odot}$.
The mass of star 1,
using light-curve solved surface gravity estimation log $g$=4.4$\pm$0.25dex,
can be estimated to be $M_1=0.08^{+0.04}_{-0.02}M_{\odot}$.
If the errors of parallax, temperature and gravity are
jointly considered, the mass estimation uncertainty would be larger, which will be discussed in Section\ref{sec.sum}.

As discussed by \citet[][]{2021MNRAS.508.4106E},
the radius estimated with SED fitting could be an upper limit,
since the light contribution from  the compact companion is ignored.
 Assuming the companion is a White Dwarf, the light contribution is very small,
on the order of a few percents, as discussed above.
The  difference of the $T_{\rm eff}$ of the primary, introduced by fitting the SED with two component, is about 40K, which will in turn lead to the difference of the radius of about 0.003$R_{\odot}$. So the effect of hot WD secondary is not important in the radius determination.

\begin{figure}[htbp!]
\center
\includegraphics[width=0.48\textwidth]{sed_fit_70904216.eps}
\includegraphics[width=0.48\textwidth]{sed_fit_70904216_double.eps}
\caption{
The upper panel: the SED fitting of ID70904216 with single component.
The KURUCZ model is used.
The red dots denote observations used for fitting,
including GALEX, SDSS u, the corrected PS1, VISTA, and WISE observations.
The red vertical lines connecting observations
denote the bias direction with respect to the model,
and the lengths are coded according to the degree of deviation.
The model parameters are $T_{\rm eff}=7440K$, log $g=4.40$ and [Fe/H]=0.08,
and the E(B-V) is 0.05.
The NUV, g, r, J and H observation are lower than the model,
while u, z and Ks are stronger than the model,
all within 1 to 3 times observational errors.
The lower panel: the SED fitting of ID70904216 with an additional WD component.
The Koester WD model is used.
The green line denotes the error of the FUV error.
Due to the large error of the additional FUV point,
direct fit cannot give instructive constrain on the WD component.
The WD component is chosen to have $T_{\rm eff}=18000K$, log $g=6.0$ and radius $\approx0.008R_{\odot}$, for illustration, the corresponding $T_{\rm eff}$ of the ELM-WD is 7400K.
}
\label{fig.sedfit}
\end{figure}

\begin{figure}[htbp!]
\center
\includegraphics[width=0.42\textwidth]{sed_teff_ebv.eps}
\caption{
The correlation between temperature and extinction in SED fitting of ID70904216.
Different lines are described in the image and are discussed in the text.
}
\label{fig.sed_teff_ebv}
\end{figure}

\subsection{Orbital parameters}
\label{sec:orbit}

The RV data from both LAMOST and P200,
as shown in Table \ref{tab.sp_obs},
is used to solve the orbital parameters.
The period is set to 0.219658 days and eccentricity is fixed to 0,
making the fit actually a sinusoidal curve fit.

The exposure time for spectral observation is 20-30minutes,
which is relatively long comparing to the orbital period 5.3 hours.
The long exposure time will lead to the phase smearing effect,
which will lower the RV amplitude.
Assuming a circular orbit, the smearing effect can be approximated by
\begin{equation}
     V(\phi)-V_0=(V_{obs}-V_0) \cdot 2\pi\delta\phi/ \sin(2\pi\delta \phi),
    \label{eqsmear}
\end{equation}
where $V(\phi)$ is the actual velocity at phase $\phi$,
$V_{obs}$ is the measured velocity from the spectrum,
$V_0$ is system velocity of the binary and $\delta \phi$ is the
half length of the exposure time in phase space.
For LAMOST,  the half exposure length is $\delta \phi\approx1800s/2P=0.0474$ in phase,
then we have amplitude scaling factor $2\pi\delta\phi/\sin(2\pi\delta\phi)=1.015$.
As for the case of P200, the 1200s exposure time corresponds to scaling factor of 1.007.
A preliminary fitting results, using observed RV without  correction, are
$K1\approx314.5km/s$ and $V0\approx-70.7km/s$.
 The phase smearing corrected RV is shown
in the `RVCorr' column of Table \ref{tab.sp_obs}.
Then we redo the fit with the corrected RV, the revised velocity amplitude
are $K1=317.33\pm2.25km/s$ and system velocity $V0=-70.31\pm1.75km/s$,
as shown  in Fig. \ref{show.fig} and Fig. \ref{fig.rvfite0}.

\begin{figure}[htbp!]
\center
\includegraphics[width=0.48\textwidth]{K1_V0_E0_70904216.eps}
\caption{MCMC RV fitting results when
the period is set to 0.219658 days and eccentricity is fixed to 0.
The returned K1 is $317.33\pm2.25km/s$
and V0 is $-70.31\pm1.74km/s$.
}
\label{fig.rvfite0}
\end{figure}

Substitute the estimated orbital period P and radial velocity amplitude K1 into equation\ref{eqmass},
the binary mass function  is,
\begin{equation}
    f(M) = \frac{M_{1} \, q^3 \, \textrm{sin}^3 i} {(1+q)^{2}} = \frac{P \, K_{1}^{3} \, (1-e^2)^{3/2}}{2\pi G}  = 0.73M_{\odot},
    \label{eqmass}
\end{equation}
where $M_{1}$ is the mass of the primary,
$q = M_{2}/M_{1}$ is the mass ratio,
and $i$ is the system inclination.
Assuming an edge-on orbit and $M_{1}$=0.08$M_{\odot}$, the least mass of $M_{2}$  would be 0.87 $M_{\odot}$, which will be about 1 mag brighter than star 1 and will dominate the spectra, if it's a normal star. Thus the companion should be a compact star. i.e., a white dwarf or a neutron star.

\subsection{Light curve fitting with WD code}
\label{sec:wdfit}

\begin{table*}
\caption{Summaries of parameters for ID70904216
\label{tab.wdfit}}
\setlength{\tabcolsep}{4.5pt}
\begin{center}
\begin{tabular}{cccc}
\hline\noalign{\smallskip}
Name & Description & Unit & Value \\
\hline\noalign{\smallskip}
RA & Right Ascension J2000 & [degrees] & 340.169878411 \\
DEC & Declination J2000 & [degrees] & -2.125739518 \\
P & Orbital Period & [days] & 2454000.0198(5) \\
T0 & Heliocentric Julian Day & [days] & 0.219658(2) \\
V0 & System velocity & [km/s] & $-70.31\pm1.74$ \\
K1 & RV semi-amplitude & [km/s] & $317.33\pm2.25km/s$ \\
\hline\noalign{\smallskip}
Plx & Parallax & [mas] & $0.72594\pm0.08538$ \\
D & Distance & [pc] & $1377.5^{+183.6}_{-145.0}$ \\
DpcLog & $log_{10}(Distance)$ & [pc] & 3.1391 \\
E(B-V) & Reddening in B-V color & [mag] & 0.05$\pm$ 0.001 \\
Ag & Extinction in g band & [mag] & 0.185 \\
Ar & Extinction in r band & [mag] & 0.136 \\
Ai & Extinction in i band & [mag] & 0.102 \\
AG & Extinction in Gaia G band & [mag] & 0.138 \\
ALB & Bolometric albedos & [-] & 0.5 \\
GR & Gravity Darkening exponent & [-] & 0.3 \\
CALIB g & g band zero point & [$erg s^{-1} cm^{-3}$] & 0.49875 \\
CALIB r & r band zero point & [$erg s^{-1} cm^{-3}$] & 0.288637 \\
CALIB i & i band zero point & [$erg s^{-1} cm^{-3}$] & 0.195711 \\
\hline\noalign{\smallskip}
$T_{\rm eff}$ & Spectral temperature & [K] & 7361$\pm$150 \\
log $g$ & Spectral surface gravity & [dex] & 4.14$\pm$0.25 \\
$\left[{\rm Fe/H}\right]$ & Spectral metallicity & [dex] & 0.08$\pm$0.15 \\
$T_{\rm eff}$ & SED fitted temperature & [K] & 7400$\pm$100K \\
\hline\noalign{\smallskip}
T1 & Light curve temperature & [K] & 7400$\pm$100 \\
M1 & Primary mass & [$M_{\odot}$] & 0.08$\pm$0.01 \\
R1 & Primary radius & [$R_{\odot}$] & 0.29$\pm$0.01 \\
log $g$  & Light curve surface gravity & dex & 4.40$\pm$0.04 \\
SMA & Semi major axis & [$R_{\odot}$] & $1.55^{+0.07}_{-0.03}$ \\
INC & Orbital Inclination & [degrees] & $76.42^{+9.74}_{-10.43}$ \\
M2 & Secondary mass & [$M_{\odot}$] & $0.94^{+0.15}_{-0.06}$ \\
\hline\noalign{\smallskip}
\end{tabular}
\end{center}
\smallskip
\end{table*}

As in Fig. \ref{show.fig},
the ellipsoidal variation dominants all the folded light curves.
The tidally distorted light curves offer a better constraint on the mass ratio and radius of the primary than the low resolution spectra\citep[][]{2012ApJ..74942}.
The WD code \citep[][]{1971ApJ...166..605W} is used
to model the ZTF g, r and i band light curves simultaneously.
The WD code atmosphere model uses SDSS filters,
which are different from ZTF g r and i filters.
But since the ZTF magnitudes are calibrated to Pan-STARRS system\citep[][]{2019PASP..131a8003M},
ZTF magnitudes are converted to SDSS using the PS1 to SDSS  relation\citep[][]{2012ApJ...750...99T}.
The  multi-color light curves also offer an independent solution of the temperature of the visible star other than the spectra and SED fitting.

The invisible compact secondary (star 2) is modeled
by setting a very large potential ($\Omega_{rm 2}$),
which will ensure an extremely small radius,
and temperature of 18000K from Section \ref{sec:sedfit}.
The limb darken coefficients are internally determined
by WD following the square root law.
The gravity darkening exponent $GR$ is between 0.2 and 0.6 in the
temperature range of 6300 and 8000K\citep[]{2017A&A...600A..30C,2021MNRAS.505.2051E}.
If we set $GR$ as a free parameter, the result
converge at $\sim 0.3$. So we first adopt 0.3 for the current calculation and further extend to 0.5 and 0.7 to test
their effect on mass determination.
Other parameters such as the
the bolometric albedos $ALB$,
the extinction in g,r and i band, and the distance ($\log pc$)
are listed in Table\ref{tab.wdfit}.
The phase folded ZTF light curves were then solved with WD code.
The calibration fluxes $CALIB$ for g, r, and i bands,
in unit of $erg s^{-1} cm^{-3}$,
are 0.49875, 0.288637 and 0.195711, respectively
\footnote{http://svo2.cab.inta-csic.es/svo/theory/fps3/index.php}.
The free parameters include
the temperature of the primary $T1$,
the mass ratio $q=(M_2/M_1)$,
semi-major axis $SMA$,
inclination angle $INC$,
and the potential of the visible star $\Omega_{\rm 1}$.

The light curve fitting result is shown in Fig.\ref{fig.ztfgri_fit} and Table\ref{tab.wdfit}.
The best fit model light curves with different inclination angles, from
60$^{\circ}$ to 90$^{\circ}$ with a step of 10$^{\circ}$, are illustrated.
In Fig.\ref{fig.ztfgri_fit}, the red color is for small inclination angle,
while the blue is for large inclination angle.
As the inclination angle changes, the mass ratio changes, then potential and orbital distance will make a compensatory change to fit the light curve. So in the range of inclination,
the difference in the light curve(0.1\%) is indistinguishable under the current photometric accuracy.
If the inclination angle is smaller ($\leq 60^{\circ}$),
the primary will overfill its Roche lobe,
accreting onto the compact star will cause emission
in the spectra, which is not seen in the spectra spanning  5 years.
While for inclination larger than $80^\circ$, the occultation of star 2 will cause a eclipse in the light curve, the depth of the eclipse depends on the temperature of the hot white dwarf, as illustrated in the inset of  Fig.\ref{fig.ztfgri_fit}.
As could be estimated from the mass function(i.e. equation\ref{eqmass}), when
the inclination is larger than $80^{\circ}$,
M2 varies from 0.84 to 1.00 $M_{\odot}$,
the corresponding radius is approximately 0.01 to 0.008$R_{\odot}$
\citep[][]{2005A&A...441..689A}.
Assuming a radius of $0.01R_{\odot}$ in the WD code (specified by $POT2$),
the eclipse depth will be most prominent in g band, which
is approximately 0.5\%, 1.5\%, 2.0\%, 4.0\%
for T2 of 12000K, 18000K, 22000K and 30000K, respectively.
When T2 is higher than 22000K, The eclipse will be deeper than 2\% in g band and will be detectable in the current data.  So if the inclination is higher than
$80^\circ$ and the companion is a white dwarf, the temperature of the white dwarf should be lower than 22000K,  this is consistent with the estimation from SED fitting.
As the eclipse is not detected, the model difference between different inclination is not distinguishable in the current data.
The upper limit of the inclination could not be determined.
Thus, we can roughly limit the angle
between 60$^{\circ}$ and 90$^{\circ}$.
Within this large inclination range,
a Monte-Carlo simulation is carried
and the result is shown in Fig. \ref{fig.ztfgri_mcmc}.
As shown in Fig. \ref{fig.ztfgri_mcmc},
the mass of star 1 (the visible star) is $M1=0.08\pm0.01M_{\odot}$,
while the mass of star 2 (the invisible compact star) is $M2=0.94\pm0.15M_{\odot}$,
indicating a possible White Dwarf nature.
The radius of star 1 is $0.29\pm0.01R_{\odot}$,
and the system separation is $1.55\pm0.07R_{\odot}$.
The temperature of star 1 is estimated to be $T1=7400\pm100K$,
which is consistent with the temperature of the SED fitting(7440K) and those from the  average of individual spectrum(7361K).
Fig. \ref{fig.ztfgri_mcmc} also shows correlations between these variables.
As inclination increases,
M1 increases,
 while M2,  system separation (SMA) and filling factor decreases.
Since both the radius and $T_{\rm eff}$ of star 1 is relatively stable,
the surface gravity log $g$  is tightly  constrained within
4.36 to 4.44 as inclination increase from 60$^{\circ}$ to 90$^{\circ}$.

To better understand the uncertainties of our solution,
we further repeated our process with larger range of
distance, extinction,
gravity darkening and reflection coefficients, and let the WD program determine the temperature  and the mass range of  star 1.
Inclination angles are chosen from 60$^{\circ}$ to 90$^{\circ}$.
The distance limit is chosen to
be 1377.5$-$145.0pc and 1377.5$+$183.6pc,
according to Section \ref{sec:distance}.
Extinction in g band  is set between 0.148 and 0.260, corresponding to E(B-V)=[0.04,0.07].
Both the gravity darkening($GR$) and reflection coefficient($ALB$) are related to the status of the envelope of the star. For convective atmosphere $GR=0.3$ and $ALB=0.5$ is suggested, while for hot radiative atmosphere(e.g., main sequence star of $T_{eff} >8000K$), $1.0$ for both are suggested.
For our case,  though the high temperature  gradient in the bloated radius of star 1 will enable a convective envelope, but to be conservative,
the following pair of values are adopted to represent the possible situation: [$GR$,$ALB$]=
([0.3, 0.5], [0.5, 0.625], [0.7, 0.75]), which are plotted in Fig.\ref{fig.m1m2error} with the blue, the cyan and the red color,respectively.

In Fig.\ref{fig.m1m2error}, the solid lines are for small extinction and
the dashed lines are for large extinction. As the  change of extinction is compensated by the temperature change(see Fig.\ref{fig.m1m2error_teff}), the radius and
the mass  constrained by the light curve keep almost constant, so the mass difference cause by extinction is negligible.
As we can see in the figure, the most critical factor is the distance.
As the distance increases, the mass(actually the radius) of star 1 will also increase.
Since the target has a relatively larger parallax error ($>10\%$),
the influence on the M1 is remarkable (100\%).
The gravity darkening and reflection coefficients
also impact the results significantly.
M1 changes slowly with the inclination angle when the distance is fixed, but
M2 is more sensitive to the inclination.
Combining all these uncertainties,
the mass of the visible star could be estimated as $M1=0.08^{+0.06}_{-0.03}M_{\odot}$,
and the mass of the invisible compact star could be $M2=0.94^{+0.45}_{-0.10}M_{\odot}$.

The change of T1 with the inclination  is plotted in Fig. \ref{fig.m1m2error_teff}.
As the inclination increases from 60$^{\circ}$ to 90$^{\circ}$, T1 increases about 50K.
For the effect of extinction, small extinction yield lower temperature (solid curves, below 7400K),
while the large extinction yield higher temperature (dashed curves, above 7400K).
This trend is similar to those of the SED fitting as in Fig. \ref{fig.sed_teff_ebv}.
As the distance increases, the temperature raises thus the luminosity raises to meet the
observed magnitude.
Different $GR$ and $ALB$ will slightly  change the temperature up to 30K.

Considering the temperature and mass within the error bar, star 1 shoud be  a helium white dwarf with bloated hydrogen envelope, and the companion  should be a high mass white dwarf or a neutron star.

\begin{figure}[ht]
\center
\includegraphics[width=0.48\textwidth]{ztfg_fit.eps}
\includegraphics[width=0.48\textwidth]{ztfr_fit.eps}
\includegraphics[width=0.48\textwidth]{ztfi_fit.eps}
\caption{Light curve fitting of ZTF g r and i band,
from top to bottom, respectively.
The grey points in the upper panel denote ZTF magnitudes,
and the curves
are models calculated with WD code,
with color from red to blue denote inclination increasing from $60^{\circ}$ to $90^{\circ}$. All the solid curve is fixed with white dwarf companion of 18000K. The fitting residuals are plotted in each lower panel,
with a standard variation of $\approx2.7$\%.
To illustrate eclipse of white dwarf occultation in the light curve, models with
white dwarfs of $12000K, 22000K$ and $30000K$  are plotted with the dotted, the dot dash and the dashed line, respectively and enlarged in the inset of each plot, while the inclination is fixed at $90^{\circ}$.
}
\label{fig.ztfgri_fit}
\end{figure}

\begin{figure*}[htbp!]
\center
\includegraphics[width=0.96\textwidth]{ID70904216_wd.eps}
\caption{
The Monte-Carlo sampling ZTF g, r and i bands, using WD code.
Diagonal elements show the probability distribution of each parameter, with percentiles of 16\%, 50\% and 84\%, denoted by vertical lines.
Note star 1 denotes the visible star,
while star 2 denotes the invisible compact star.
}
\label{fig.ztfgri_mcmc}
\end{figure*}

\begin{figure}[htbp!]
\center
\includegraphics[width=0.48\textwidth]{m1m2_errors.eps}
\caption{
The uncertainties of mass estimation,
considering distance, extinction,
gravity darkening and reflection coefficient.
The solid lines are for low extinction.
The dashed lines are for large extinction(almost coincident with the solid line).
The blue color is for $GR=0.3, ALB=0.5$,
the cyan color is for $GR=0.5, ALB=0.625$,
and the red color is for $GR=0.7, ALB=0.75$.
The plus symbol denotes the masses estimated by MCMC sampling,
which is (0.08$M_{\odot}$, 0.94$M_{\odot}$).
The circles denotes the points for inclination 70$^{\circ}$,
while the boxes denotes the points for inclination 80$^{\circ}$.
See text for details.
}
\label{fig.m1m2error}
\end{figure}

\begin{figure}[htbp!]
\center
\includegraphics[width=0.48\textwidth]{wd_inc_teff.eps}
\caption{
The variation of $T1$ in the test of Fig.\ref{fig.m1m2error}.
The color code is same as Fig.\ref{fig.m1m2error}.  The dashed lines are
for high extinction and the solid line are for low extinction.
The thick and thin lines represent  large and small distances,respectively.
See text for details.
}
\label{fig.m1m2error_teff}
\end{figure}

\section{Summaries and Discussions}
\label{sec.sum}

\subsection{Formation  of ID70904216}
\citet[][]{2019ApJ...871..148L} suggested that ELM WDs with mass less than $\sim 0.22M_\odot$ can not be produced from the CE ejection process due to the large binding energy of the progenitor envelope. Therefore, ID70904216 is supposed to be formed through stable Roche lobe overflow.
To model the evolutionary history of ID70904216, we perform binary evolution simulations by using the stellar evolution code Modules for Experiments in Stellar Astrophysics (MESA, version r12115) \citep[][]{2011ApJS..192....3P, 2013ApJS..208....4P, 2015ApJS..220...15P, 2018ApJS..234...34P, 2019ApJS..243...10P}. The standard evolutionary tracks for ELM WDs from the stable Roche lobe overflow with mass from $0.16-0.21M_\odot$ (in steps of $0.01M_\odot$ from right to left) are presented in black lines of Fig. \ref{fig.elmtracks}, where the termination of mass transfer is marked with black crosses. After the mass transfer phase, the pre-ELM WDs are in the bloat state, and the radius gradually decreases.
The comparison between observation parameters of ID70904216 and the theoretical tracks suggests that ID70904216 may have a mass around $0.160-0.170M_\odot$. The estimation of ELM WD mass is significantly larger than that in the light curve fitting results. Besides, the standard binary evolution models can not produce pre-ELM WDs with mass less than $\sim 0.14M_\odot$, as shown in previous works \citep[][]{2014A&A...571A..45I, 2017MNRAS.467.1874C, 2019ApJ...871..148L}.

If ID70904216 have a mass less than $\sim 0.14M_\odot$, the extra mass-loss mechanism for the progenitor of ELM WD is needed. For example, if the companion is a NS, the pulsar evaporation on the ELM WD progenitors can strip a part of envelope, which leads to low-mass remnants \citep[][]{2016ApJ...830..153J, 2021MNRAS.506.3323T}. Following \citet[][]{2016ApJ...830..153J}, we calculate several models with considering the pulsar evaporation effects. The corresponding mass-loss rate of the donor is given by
\begin{equation}
\dot{M}_{\rm d,evap} = -\frac{f}{v^2_{\rm d,esc}}L_{\rm p}\left(\frac{R_{\rm d}}{a}\right),
\end{equation}
where $f$ is the efficiency of pulsar irradiation, $v_{\rm d,esc}$ and $R_{\rm d}$ are the surface escape velocity and the radius of the donor, respectively, $L_{\rm p}$ is the spin-down luminosity of the pulsar, and $a$ is the binary separation. Other initial parameters are similar as that in Model A of \citet[][]{2015ApJ...814...74J}.
The results of evaporation efficiency with $f=0.1,0.2$ are shown in Fig. \ref{fig.elmtracks}. We see that the ELM WDs with mass $\lesssim 0.14M_\odot$ can be produced, where the minimum ELM WD masses for $f=0.1,0.2$ are about $0.13M_\odot$ and $0.11M_\odot$, respectively. However, the evolutionary tracks for those ELM WDs with mass $\lesssim 0.14M_\odot$ are below the observation value of ID70904216. Therefore, the formation of ID70904216 gives a challenge to the standard evolutionary models of ELM WDs, and it deserves further detailed investigations.

\begin{figure}[htbp!]
\center
\includegraphics[width=0.48\textwidth]{ID7090evolution.eps}
\caption{The evolutionary tracks of ELM WDs in $\log\; g-\log\; T_{\rm eff}$ plane. Theses tracks have the same initial donor masses ($1.2M_{\odot}$)
and accretor masses ($1.1M_{\odot}$). The standard evolutionary models of ELM WDs are shown in black solid lines with ELM masses of $0.16-0.21M_\odot$ in a step of $0.01M_\odot$. The cross symbols denote the end of mass transfer (MT) and the start of the contraction phase. Stars between the end of MT and the beginning of WD cooling track, generally referred as pre-ELMs, have nearly constant luminosity, decreasing radius and increasing temperature, and a lifetime of $\approx$ 1Gyr depending on their masses. The red lines are for the models with considering the pulsar evaporation effects. The models of $f=0.1$ are shown in the red dotted lines, where the ELMs have masses of $0.13,0.14,0.15M_\odot$ from right to left. The models of $f=0.2$ are shown in the red dashed lines, where the ELMs have masses of $0.11,0.12,0.13M_\odot$ from right to left.}
\label{fig.elmtracks}
\end{figure}

\subsection{Conclusion}

In this work, we present detailed mass estimation for ELM-WD
ID70904216, which was discovered in the LAMOST low resolution survey as a binary system with the primary star orbiting an unseen compact star  with a RV semi-amplitude of $K1=317.33\pm2.25km/s$  every 0.219658$\pm0.000002$ days. Kinematics analysis indicates that the system  is a thin disk binary.
Accurate parallax from GAIA help to constraint the primary radius to $0.29\pm0.01R_{\odot}$. Temperature from the spectral, SED and the multi-color light curve fitting  are consistent with $7400\pm100K$. The radial velocity curve combining with the ellipsoidal light curve offer a better  constraint on the gravitational potential thus the mass providing that the temperature and the radius could be accurately determined. Considering the uncertainty in the input parameters, our best estimation on mass of the visible star is $M1=0.08^{+0.06}_{-0.03}M_{\odot}$, and the mass of unseen compact star  is $M2=0.94^{+0.45}_{-0.10}M_{\odot}$.

Considering the mass and temperature of the primary star, it should be a helium white dwarf with very bloated hydrogen envelope, i.e. a pre-ELM WD, just finishing its  mass transfer and entering the constant luminosity contracting phase. We note that the star was also listed as a pre-ELM WD candidate in table D1 of  \citet{2021MNRAS.508.4106E} , but since there is no spectral observation,  no mass estimation was given in that paper.
The mass of star 1 is relatively small compared to ELM theories, as shown in Fig. \ref{fig.elmtracks}.
Yet the small mass of visible star is also in accordance with
the spectral estimated surface gravity (log $g$=4.14$\pm$0.25dex),
and the estimation from light curve fitting ($4.40\pm0.04dex$).
According to our current radius estimation,
to get a mass of $\approx0.14M_{\odot}$, a surface gravity of $\approx4.6$ is needed, which could be barely reached at the edge of our parameter estimation.
Since the visible star is almost filling its Roche lobe
(from $\approx95\%$ to $100\%$),
the mass can be estimated from radius and the  density period relation
\begin{equation}
\overline{\rho}_{donor} \approx 0.185 g{cm}^{-3}(P_{orb}/day)^{-2},
\end{equation}
with an accurate of 6\% \citep[][]{2022MNRAS.511L..24E}.
Using $R_1=0.29\pm0.01R_{\odot}$ and period of 0.219658 days,
the mass of star 1 is $0.060\pm0.006M_{\odot}$.
This can be used as an auxiliary verification.

The invisible companion has a mass of $0.94^{+0.45}_{-0.10}M_{\odot}$,
indicating a candidate of massive White Dwarf or a Neutron Star.
As no significant X-ray observation is found,
radio observation may be used to verify if it is a pulsar,
and deep ultraviolet spectral observation may be used to verify if it is a White Dwarf.
If it is a white dwarf, the temperature should be lower than 22000K based on the ultraviolet photometry of GALEX.
A high cadence photometry with precision of 0.5\% will also be help to discern the shallow eclipse of a white dwarf.
Besides, the resolution and SNR of current LAMOST and P200 spectra are too low to tell the chemical character of the primary.
High resolution spectral observations, using larger telescopes,
in the optical and near infrared bands, may reveal  clues on the
evolution history of ID70904216.

\section*{acknowledgements}
Guoshoujing Telescope (the Large Sky Area Multi-Object Fiber Spectroscopic Telescope LAMOST) is a National Major Scientific Project built by the Chinese Academy of Sciences. Funding for the project has been provided by the National Development and Reform Commission. LAMOST is operated and managed by the National Astronomical Observatories, Chinese Academy of Sciences.
This work presents results from the European Space Agency (ESA) space mission Gaia. Gaia data are being processed by the Gaia Data Processing and Analysis Consortium (DPAC). Funding for the DPAC is provided by national institutions, in particular the institutions participating in the Gaia MultiLateral Agreement (MLA). The Gaia mission website is https://www.cosmos.esa.int/gaia. The Gaia archive website is https://archives.esac.esa.int/gaia. We acknowledge use of the VizieR catalogue access tool, operated at CDS, Strasbourg, France, and of Astropy, a community-developed core Python package for Astronomy (Astropy Collaboration, 2013). This research made use of Photutils, an Astropy package for detection and photometry of astronomical sources.
Z.H.T. thanks the support of the National Key R\&D Program of China (2019YFA0405000), NSFC 12090041 and NSFC 11933004.
Y.H.L. acknowledges support from the Youth Innovation Promotion Association of the CAS (Id. 2020060).
ZWL and XFC thanks the support of National Key R\&D Program of China (Gant No. 2021YFA1600403), National Natural Science Foundation of China (Grant Nos. 11733008, 12103086, 12090040/12090043, 12125303) and the Yunnan Fundamental Research Projects (No. 202101AU070276).
We also acknowledge the science research grant from the China Manned Space Project with No.CMS-CSST-2021-A10.

\bibliographystyle{aasjournal}

redpajama_set_name: RedPajamaArXiv


text:
Plant Your Feet: Reebok Launches Sneakers Made From Corn, Cotton
August 21, 2018 | By Amanda Ellis
To kick off its sustainability line, Reebok unveils the shoe industry's first corn-based footwear.
Eco-friendly apparel is on the rise. Brands are implementing creative ways to reduce environmental impact — and footwear is no exception. Reebok's Cotton + Corn sneakers represent the latest step forward toward solving the shoe industry's sustainability problem.
"Green" footwear is not a new trend. In May 2017, VIVOBAREFOOT partnered with Bloom on running shoes completely made of algae. And Allbirds crafts its footwear from wool. Launched this month, these sneakers mark the first time we've ever seen shoes made from corn.
Reebok Cotton + Corn
Reebok's Future team launched the Cotton + Corn initiative last year while hinting at creating the world's first compostable shoe. While they haven't quite hit the mark, Reebok's NPC UK C&C sneakers are the closest thing out there.
"Most athletic footwear is made using petroleum to create synthetic rubber and foam cushioning systems," said Bill McInnis, head of Reebok's Future team, in a release. "With 20 billion pairs of shoes made every year, this is not a sustainable way of making footwear."
According to McInnis, designers at Reebok sought out plant-based alternatives to oil-based mainstays. And the result, the brand claims, is a sneaker that "performs and feels like any other shoe."
NPC UK C&C Sneakers
Instead of oil, Reebok started with things that grow. It partnered with DuPont Tate & Lyle Bio Products, a bio-based solutions company. Together the companies developed Susterra propanediol, a petroleum-free product derived from industrial-grown corn. This material comprises the sole while the upper sports 100 percent cotton.
Reebok then integrated insoles derived from castor bean oil and used no dyes to make the NPC UK. To round it off, the company wraps each pair of shoes in 100 percent recycled packaging.
The result is a 75 percent USDA-certified bio-based shoe. While wearing plants on your feet might make you feel good, surprisingly, they also look good.
To be sure, these aren't high-performance runners just yet. But the combination of sustainable materials and everyday sneaker aesthetic suggest Earth-friendly technical footwear may be on the horizon.
Does Eco-Friendly Fit Everyone?
The majority of modern consumers care about the environment, but it's important to make of note of these sneakers' unisex feature. While unisex sizing simplifies production, it could be an issue in terms of fit.
Reebok lists a women's size conversion chart on the product page (alluding to standard men's sizing), but we have yet to see how this eco-minded alternative stacks up for comfort.
Reebok: Growing the Future of Shoes
The iconic shoe brand has indicated this is just the beginning of the Cotton + Corn initiative, with a broad selection of bio-based footwear yet to come. And the sticker price, $95, looks to attract a wide audience. It's within the budget of most shoe-shoppers, so this is one eco-alternative that also targets mainstream consumers.
And so far, the demand has been high. Reebok's site states the NPC UK Cotton + Corn sneakers are sold out. If you want to get your hands (and feet) on a pair, you can sign up for notifications when they become available.
Reebok is officially "growing shoes." After the release of the NPC UK C&C sneakers, there's no telling what kind of plant you'll be able to wear next.
Topics: Footwear
Up Next: Why This Champion Marathoner Says Running Shoe Stores Are Off Track
Why This Champion Marathoner Says Running Shoe Stores Are Off Track
5 Ways to Rock the Modern Hiking Boot


text:
Qshell is an optional command-line interpreter (shell) for the IBM i operating system. Qshell is based on POSIX and X/Open standards. It is a Bourne-like shell that also includes features of KornShell. The utilities (or commands) are external programs that provide additional functions. The development team of Qshell had to deal with platform-specific issues such as translating between ASCII and EBCDIC. The shell supports interactive mode as well as batch processing and can run shell scripts from Unix-like operating systems with few or no modifications.

Commands
The following is a list of commands that are supported by the Qshell command-line interpreter on IBM i 7.4.

Differences from other Unix shells
Qshell does not support the  redirection operator or provide a command history. It also has no job control support as IBM i operating system does not have the concept of a foreground or background process group. The POSIX standard  and  built-in commands are therefore not available as well.

Compared to PASE for i
According to IBM, QSHELL is a "Unix-like" interface built over IBM i.  The commands issued by the user point to programs in a "Qshell" library. It began as a port from the ash shell, which was a Bourne-like shell created by Berkeley Software Design.

See also
Control Language
Comparison of command shells

References

Further reading

External links

Exploring iSeries QSHELL

Command shells
Interpreters (computing)
IBM operating systems

redpajama_set_name: RedPajamaWikipedia


Fuel price drop: Petrol costs Rs 83.72 per litre in Mumbai, Rs 78.21 per litre in Delhi. Prices of fuel in Delhi and Mumbai witnessed yet another drop.
The prices of petrol and diesel in Delhi and Mumbai witnessed yet another drop on Thursday. Notably, petrol prices were slashed by Rs 0.21 and Rs 0.20 in Delhi and Mumbai respectively. A reduction was also witnessed in diesel prices by Rs 0.18 and Rs 0.19 respectively.
Following the reduction, petrol is being sold at Rs 78.21 per litre in Delhi and Rs 83.72 per litre in Mumbai. Diesel is being retailed at Rs 72.89 per litre and Rs 76.38 per litre in Delhi and Mumbai respectively.
The price of petrol in Kolkata was slashed to Rs 80.13 while that of diesel was at Rs 74.75. In Chennai, the price of petrol was Rs 81.24 and that of diesel was Rs 77.05.


Dosharon is dedicated to solving challenging supply and procurement problems, while creating measurable and meaningful value for its customers, employees and shareholders.
Many of today's supply chains and operations are too inflexible to give individual customers the hyper-personalized experience they want from the suppliers.
Businesses struggle to compete with emerging players better equipped to handle digital disruption. We are disruptors in the supply and service industries because of our systems, solutions and the ability to tailor our services to customer needs.
Dosharon is dedicated to solving challenging supply, service and procurement problems, while creating measurable and meaningful value for its customers, employees and shareholders.
To be the most preferred partner in the supply industry by integrating customers' systems to our supply solutions.
Our main objective is to ensure that our clients get the lowest possible price for their desired quality and deliver the right product and service. We source vendors, certify factories and products, monitor production and inspect final goods.


I found your hotel through Tripadvisor and your hotel seems clean and awesome.
I am going to Delhi for 10 days more or less and will not be there till Tuesday (20 Sep,2016).
I am a single man and need a single bed room there.
Could you let me know your price details so that I can consider about it?


text:
"""
WSGI config for holiday_planner project.

It exposes the WSGI callable as a module-level variable named ``application``.
"""
import os
from os.path import abspath, dirname
from sys import path

SITE_ROOT = dirname(dirname(abspath(__file__)))
path.append(SITE_ROOT)

os.environ.setdefault("DJANGO_SETTINGS_MODULE", "holiday_planner.settings")

from django.core.wsgi import get_wsgi_application
application = get_wsgi_application()  # pylint:disable=invalid-name

redpajama_set_name: RedPajamaGithub


Social networking sites – online platforms for communicating with people has become an important part of our lives. In the 21st Century, it doesn't matter what your age is, but having an account on social media sites like Facebook, Twitter, LinkedIn, etc. is essential to communicate with others.
Over the years, the popularity of such sites has increased with the growing population because these sites are able to meet the needs and interest of many people. For teens and adults, it is a way to socialize while for professionals it helps in growing their businesses.
Social networking sites benefit in many ways, however overlooking the risks involved with them would be a foolish choice. Every day we hear threats of criminal activity like identity theft, hacking and injecting malware/viruses via photos, videos, also emoticons and GIFs.
As a result, users fall prey to impersonators causing damage to their accounts while disrupting the total security of Windows and Mac computers. To make out the best online use of social networking sites, it is important to avoid the risks of staying secure by using a free anti-virus: ITL Total Security & Antivirus.
Thus, users need to understand and Follow 5 Tips to Stay Secure on Social Networking Sites for highly effective and secure use.
Nearly all the social networking sites have a pre-set of default privacy settings. Majority of people often feel that these default privacy setting are sufficient enough to save your profile information from online scammers. But, it is not true!
Social networking sites give many options for privacy settings from blocking strangers to select which and what kind of information do you want to show. The settings limit the shared information and more you open your account to the public, higher the chances of criminal activities increases.
It is easy to adjust social media privacy settings any time and one should always keep their accounts connected to email id and phone number.
On a social networking website, people have options of sharing their personal details with friends and followers, even more, they could share it publicly. Sharing required information is okay, but revealing every facet of your life may put you in trouble.
For the sake of your personal safety, you must not reveal your date and place of birth, address and phone number, as this had put several people into the severe risk for identity thefts and fraud.
The basic personal information is also required to sign up on social media sites but after you sign up, you have the options to make this information private.
Additionally, it is extremely important that one mustn't reveal their credit card numbers, banking details, passwords or social security numbers, OTP pins, etc. on any networking site.
If you share all such information, it will make you a victim to the crimes ranging from stalking to identity theft and frauds. We also suggest you control the information you share outside with other sources. Do not share your personal details.
Microblogging on social networking sites allows users to share their every moment of life and happiness. It is mainly done to get a social attraction that helps in building a strong social media interaction.
But revealing too much about your personal life would make you an easy victim of cyber attackers, ethical hacking and social hijacking. It is better to reveal less and stay grounded!
There exist a number of reasons for anyone to put up a false account. Such accounts are set up to misrepresent themselves in front of another person for making false statements.
If there is ever an uncertainty about the authenticity of any account in your friend list, then it is important enough to check the individual. If the account is found suspicious, then one must block it.
In order to ensure the security of your own account, one must review their profile once in a week to check the settings, content shared and people who liked you, followed you and pretty much stalking you.
Security is very important for anyone's social networking account same like computers and other devices. Creating a strong password will always prevent hackers from gaining access to your account.
Always create a password which is greater than eight characters to secure social media accounts. The characters must contain letters, special symbols and numbers. Also, it must be changed in every three months.
Be selective while accepting friend requests.
Always set few security questions and answers.
Social media accounts are regularly hacked via malicious links. Always be careful to click links.
Control your commenting and stop yourself from giving online comments publicly.
Do not ever violate social networking social media privacy policies.
Create a small but genuine social network.
Keep track of your social media activities.
Have the best security anti-virus like ITL Total Security to make your online presence safe.
We live in a world where social media is useful and advantageous. The culture of sharing information is important but one must realize not to share everything on social networking sites.
You never know what can go wrong due to any of your public activity. As far as cyber-security is concerned, it is definitely important to follow 5 tips to stay secure on social networking sites.
However, the best option is to follow a free anti-virus tool like ITL Total Security that has the capability to stop incoming of the malicious file into your computer.
The above tips will help you to stay secure by yourself at the personal front, but the tool will work 24X7 to safeguard your online presence forever on social networking sites making everything easy and threat free.


text:
Len Cormier (1924 – June 16, 2008) worked for many years in the U.S. aerospace industry, in government, large industry, and as a private entrepreneur.
He developed many creative proposals for reusable launch vehicles, and was present at several key events of the early Space Age.

Early life and career
Len Cormier was born in 1924 in Boston, Massachusetts.
After learning to fly in the Second World War,
he became a U.S. Navy fighter pilot, and executive officer of an ASW patrol squadron.
He obtained a B.A. in physics from Berkeley in 1952.
"He joined the Navy Reserve in 1947
and achieved the rank of lieutenant commander in 1958. He retired from
the reserves in 1966." He spoke Russian and English.

Involvement with the International Geophysical Year
In 1956 he began work at the National Academy of Sciences (NAS) of the U.S.A. As a staff member there in 1957 he was involved in work on a satellite to be launched as part of the International Geophysical Year (IGY), 1957–1958, and on publication of IGY scientific results.

He attended the October 1957 conference at which the Soviet Union hinted at the upcoming launch of Sputnik 1. According to his family, this event "made a tremendous impression on him".

In 1958 he was present at the Jan. 31[?] press conference at the National Academy of Sciences
following the launch of the first US satellite, Explorer 1.
While at the NAS he was also involved with the Moonwatch, Moonbeam and Phototrack volunteer groups supporting the IGY satellite program.

Later work
In 1959, he moved to NASA headquarters, where he was involved with the work of the Space Science Board.

Around 1960 he left NASA to work at North American Aviation, where he was project engineer for
space transportation systems at the Los Angeles Division for several years.

Private entrepreneur
In 1967 Cormier formed a company called TranSpace, marking the beginning of his work on a commercial approach to spaceflight, which continued for the remainder of his life.
Later TranSpace became Third Millennium Aerospace, Inc. Other companies he set up included PanAero, Inc. However Cormier struggled to obtain sufficient investment for his Space Van (and other) concepts, which underwent many revisions over the years.

Concerned with the economics of commercial space transportation with several papers on the topic published by the AIAA. Cormier was a charter member and a reappointed member of the Department of Transportation's Commercial  Space Transportation Advisory Committee (COMSTAC), providing advice to the FAA.

He designed and advocated many reusable launch vehicles (RLVs):

 Space Van was intended to carry sixteen passengers, plus crew, to a 40-degree low Earth orbit for $3,000,000 per flight in 1996 dollars.
 Cormier's Bantam Boosters, Millennium Express. The smaller Bantam Van would carry a 400 kg payload. This reflected his belief a small RLV was essential to obtaining appropriate returns on investment.
 Bear Cub using a Tupolev Tu-95 "Bear" bomber as the launch platform for a liquid-fueled rocket.
 His PanAero company was an Ansari X PRIZE contestant, with their SabreRocket entry based on an existing Sabre-40 jet.
 PanAero later unsuccessfully proposed Space Van 2010 in response to NASA's COTS proposals in March 2006.

Cormier was a frequent poster to Usenet's sci.space.* and other newsgroups for more than
10 years .
For his work towards low-cost reusable spaceflight he was nominated for the Heinlein Prize.
Cormier died a well-respected member of the private spaceflight community on 2008-06-16, aged 82.

Partial list of works
 Cormier, L.  Millenium Express, AIAA 2001-3962, 37th AIAA/ASME/SAE/ASEE Joint Propulsion Conference, 8–11 July 2001, Salt Lake City, Utah.
 Cormier, L.  X Van Economics, AIAA-98-3954, 34th AIAA/ASME/SAE/ASEE Joint Propulsion Conference, July 13–15, 1998, Cleveland, Ohio.
 Cormier, L.  Bantam Boosters: The Key to Small RLVs?, AIAA-97-3124, 33rd AIAA/ASME/SAE/ASEE Joint Propulsion Conference, July 6–9, 1997, Washington State Convention and Trade Center, Seattle, Washington.
 Martin J.A. and Cormier L., Where profit drives RLV, AEROSPACE AMERICA , Vol.35, Iss. 4, pp 40–42. April 1997.
 Cormier, L. The Economics and Technical Benefits of the Assist-Stage Concept for Space Launch, AIAA-96-2773, 32nd AIAA/ASME/SAE/ASEE Joint Propulsion Conference, July 1–3, 1996, Walt Disney World Dolphin, Lake Buena Vista, Florida.
 Cormier, Leonard N. Simplified satellite prediction from modified orbital elements (Washington, National Academy of Sciences, IGY World Data Center A, Rockets and Satellites, 1959.)
 Berkner, Lloyd V., Gilman Reid, John Hanessian Jr., Leonard Cormier. Manual on rockets and satellites, vol. 6, Annals of the International Geophysical Year. (Pergamon, 1958.)

Awards and honors
 Member of the American Institute of Aeronautics and Astronautics.
 Nominated for the Heinlein Prize.

References

American aerospace engineers
NASA people
1924 births
2008 deaths
20th-century American engineers
United States Navy pilots of World War II
University of California, Berkeley alumni
United States Navy officers
United States Navy reservists


text:
Cladomyza microphylla är en tvåhjärtbladig växtart som först beskrevs av Carl Karl Adolf Georg Lauterbach, och fick sitt nu gällande namn av Danser. Cladomyza microphylla ingår i släktet Cladomyza och familjen Amphorogynaceae. Inga underarter finns listade i Catalogue of Life.

Källor

Sandelträdsordningen
microphylla


Child Youth and Family Mental Health provides tertiary services to children, youth and their families throughout Vancouver Island and the Gulf Islands. This specialized intervention is for children and youth whose chronic and often acute mental health needs have exceeded the capacity of community resources, including the Ministry of Child and Family Development.
We are unable provide long term treatment services, respite services or residential placements.
Referrals for elective admissions to Anscomb Outpatient Services, Ledger House, the Central Island Child and Adolescent Psychiatry Program and the Collaborative Psychiatric Outreach Program must meet eligibility criteria for a tertiary level service. This means that clients have already received assessment and intervention services in the community.
Referrals are regularly reviewed by the Intake Review Committees. The Committees consist of psychiatry, administrative staff and the intake clinicians. A decision is made to either accept the child/youth for the appropriate waitlist, or to decline the referral and make alternative recommendations for other resources or services.
Complete the Ledger House Referral Form or Child, Youth and Family Mental Health Services Referral Form and fax to 250-755-7946.
Requests for urgent Ledger House inpatient admissions can be made directly by phoning (250) 519-6720.
To discuss a potential referral, or obtain more information on any of our services, please contact our intake service at 250-519-6756.


text:
Home › Rob reads › Interesting reads
By The bored journalist on September 9, 2019 • ( 0 )
Men paid 9.9% more than women
With just hours to go before the deadline for UK companies to report their gender pay data, the latest figures show that men are paid on average 9.9 per cent more than women in Britain. Under rules introduced last year, UK employers with 250 or more workers are required to report the difference between what they pay men and women. The deadline for public sector employers passed at midnight on Friday, while the cut-off for private sector companies is midnight on Wednesday.
Forcing employers to reveal their gender pay gaps is making them think
BRITAIN has one of the widest gender pay gaps in Europe. For every pound that men earn, women make 80p, and the disparity has moved little in 15 years. Vowing to end this "scandal" within a generation, in 2015 the then prime minister, David Cameron, pushed through a policy long resisted by businesses. Organisations with 250 or more employees would have to publish the gap in hourly pay between men and women. April 4th 2018 was the deadline for the first wave of this annual exercise. The results aren't pretty.
Norway's invisible glass ceiling
OSLO — When it comes to promoting women's careers, Norway is often held up as a model. The country has been described as one of the "most gender equal nations in the world." And its state-mandated quotas of women on company boards have been put forward as an example for other countries to follow.But if you look — as I have — at the percentage of women who reach the top of the career ladder, another picture emerges. By this standard, Norway is not much of an exemplar. It ranks just above Romania and Germany, and far behind countries like Russia, the United States, France and Latvia.
Why Gender Equality In The Workplace Is Not Enough
Most organisations recognise the benefits of having a gender diverse workplace in the modern economy—equal hiring practices lead to higher engagement, more creativity, and better talent recruitment. But are there benefits that go beyond equal numbers of men, women, and gender-diverse people in the room?
‹ What I thought of The secret Life of Pets II
In the News: 09-09-2019 ›
Categories: Rob reads
Tags: #articles, #interesting, #news, #reading


Stephanie Teaching in the GreenhouseIn August, The Food Project embarked on its second year as the Massachusetts host site for FoodCorps, a national nonprofit organization that works with schools to create a healthier school food environment. What follows is the first of a series of blogs profiling the FoodCorps members who are serving at The Food Project during the 2012-13 school year.
"There's no [competition] to the flavor of something that is fresh and was just picked," says FoodCorps service member Stephanie Simmons. "I think that's why a lot of kids don't like vegetables - because they haven't had a chance to taste them at their best."
The Community BayWhile many of Massachusetts' farms are harvesting their last crops of the season and preparing for rest, the Dudley Greenhouse is just starting to blossom. Food Project staff and community members spent the month of September welcoming new partners to the greenhouse and preparing for a winter of delicious vegetables.
In July, the Dudley Greenhouse received 18 applications from groups looking to grow food and learn together in the greenhouse's community bay. The greenhouse advisory group selected eight groups to share space and resources in the greenhouse during the upcoming year. The new groups include local elementary schools, community gardeners, and refugee groups. Each week, FoodCorps Service Member Marlie Wilson welcomes second and third grade classes from Mason and Winthrop Elementary Schools to the greenhouse to learn to grow food and explore gardening, nutrition, and plant science.
October 16 - also known as World Food Day - marked the start of nearly two weeks of events here in Boston and around the country to highlight the wealth of activities and opportunities around food in our communities. On Tuesday evening, TFP Director of Community Programs Brandy Brooks joined Vivien Morris of the Mattapan Food and Fitness Coalition and Karen Spiller of the Boston Collaborative for Food and Fitness for a roundtable discussion on urban agriculture and food justice hosted by Common Boston.
(Courtesy Sacha Pfeiffer/WBUR)The Food Project's efforts in the Dudley neighborhood to address the presence of lead in local soil – and increasingly in some of the compost available to community gardeners – was featured in a report broadcast on WBUR, Boston's National Public Radio news station.
Kathleen Banfield, TFP's community programs coordinator, and Dan Brabander, a geochemist at Wellesley College, talk about this complicated issue and what gardeners in the area can do to keep their gardens safe.
For more information, check out this article about the work of Professor Brabander and his research students at Wellesley College.
Giving Common Challenge Starts Soon!
On Wednesday, October 10 and Thursday, October 11, The Food Project will be participating in The Boston Foundation's Giving Common Challenge. The Giving Common Challenge is a 36-hour online event to drive donations to participating nonprofits. From 8:00 a.m. on Wednesday to 8:00 p.m. on Thursday, Food Project supporters can donate to us through our profile on the Giving Common website. In addition to the donations collected, The Boston Foundation is offering $150,000 in prizes to participating organizations for various accomplishments, such as most money donated during particular time slots or the highest number of unique donors. Please check out our Giving Common profile and help us win some prizes! Gifts of any size are appreciated - from $25 to $5,000!
Food Day is a nationwide celebration of and movement toward more healthy, affordable, and sustainable food. Join your community for this series of events and day of action on October 24! Food Day aims to bring us closer to a food system with "real food" that is produced with care for the environment, animals, and the women and men who grow, harvest, and serve it. On October 24, thousands of events will take place across all 50 states to celebrate.


August 2017 – DriTac Flooring Products is introducing a line of eco-friendly, acoustical abatement underlayment for residential and commercial flooring applications: DriTac 8301 Impact 1mm for resilient flooring installations and DriTac 8302 Double Impact 2mm for wood and laminate flooring installations.
These lightweight flooring underlayments incorporate DriTac's Total Sound Reduction System (SRS) complete with a lifetime warranty when used in conjunction with approved DriTac flooring adhesives in 'double-stick' applications. DriTac's SRS was developed with dual force, silent-fuse technology, affording customers an optimized sound abatement system covered by DriTac's single, all-inclusive warranty.
DriTac 8301 Impact and DriTac 8302 Double Impact are technologically advanced underlayments that grant exceptional sound control properties, providing industry leading footfall performance with anti-crush technology designed to attain a cushioned, quiet and comfortable flooring system. Both products are available in lip and tape and non-lip and tape versions. The lip and tape (8301LT and 8302LT) system offers a built-in vapor barrier with safeguard seaming.
DriTac 8301 and 8302 contain negligible VOC content that measures below quantifiable levels, providing the green community the best sound abatement choice for their eco-friendly projects. These underlayments exceed every standard for indoor air quality, are hypo-allergenic, mold/mildew/bacteria resistant and devoid of toxic additives.
DriTac Flooring Products, LLC is celebrating over 60 years as one of the most experienced manufacturers of environmentally friendly flooring adhesives in the market. DriTac is committed to manufacturing eco-friendly products for the flooring industry with a comprehensive line of premium "green" zero VOC and zero solvent adhesives and installation solutions that help contribute credits towards LEED certification.


Having amassed well over 30 million streams online, singer-songwriter and platinum producer is poised to add significantly to those figures this year with the release of his newest single, Professional Lovers. Named a Clear Channel "Artist to Watch," back in 2011, Jared debuted his first EP, "Falling Through Holes," with the single "It's Over (Goodbye)" to critical acclaim, breaking Top 40 in the Hot AC format, and landing the Boston native on several stages across the United States, headlining and opening for artists such as Gavin Degraw, TRAIN, Brian Mcknight and many more. With his signature soulful vocals and unmistakable falsetto, Jared quickly landed a bevy of song placements across the Television landscape, including networks such as NBC, CBS, and MTV. "It's Over (Goodbye)" and the emotionally brilliant "Beautiful World" was featured in back-to-back episodes of FOX's American Idol, introducing Jared's undeniable talents to a newly emerging, and what has proved a significantly loyal, fanbase. Recently, Jared has been writing and producing for globally renowned artists such as Jason Derulo, Jordin Sparks, Tiesto, New Kids on the Block and has been enlisted by some of the world's top DJ's including, Markus Schultz, Fedde Le Grand, Laidback Luke, Vicetone. Disco Fries, Jenaux and CLMD to write and be featured as lead vocalist on original music they have released or plan to soon release. Jared has been featured on Billboard.com, MTV.com, Artistdirect.com, PerezHilton.com, THR.com, GlobalGrind.com and several other top music and entertainment sites.


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Transcripts are official academic records of students' work at Georgia College. They are issued by the Registrar's Office upon the student's written request. Transcripts are usually mailed out within one to two working days. Additional time should be allowed for requests made at the beginning and end of each semester.
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Students and alumni may also request a transcript in person by visiting the Registrar's Office, 107 Parks Hall, between 8 a.m. and 5 p.m. Monday through Friday. A photo ID will be required.


I dashed out as fast as I could.
I saw  a window and I threw myself out the window and got up and began running for my life.
I saw people but I knew they were her demons.
So I ranned past them.
They had no eye's and their lips were in zippers.
She called out to them as I was running she said Oh heil me you're master..
Then she hollered seize him.
I ranned to this river and I jumped in a boat and got the paddles and began paddling deeper into the river.
I knew I wasn't gonna be able to get away.
And they were already splashing in the water after me.
So I beganned to pray out loud.
I prayed although I was a atheist.
I knew this was not a dream.  I knew I probably got trapped into a sleep paralysis and probably died in it.
Their arm's and part's began to fall off.
I kept praying out loud.
She let out a scream Nooo.
Then she fell to the ground.
And this white light grew nearer.
I began to dissolve and I could hear a man speak to me,  you must aways pray,  keep praying.
And he said you are saved.
And he sent me back to my body.
I awoke from the dream,  sleep paralysis.


text:
Q: Terraform Outputs: How do I create a (map?) and how do I use the map? Is a map even the right tool? I am struggling with a few terraform concepts.
I am successfully using the aztfmod/azurecaf provider to name my resourcegroup, but this means I need to get that name as an output for the companynet.resource_group module, so that I can use that name again when calling the companynet.key_vault module.
# terraform.tfvars

resource_groups = {
  rg1 = {
    name     = "resourcegroup1"
    location = "eastus"
  }
  rg2 = {
    name     = "resourcegroup2"
    location = "eastus"
  }
}

# root main.tf

provider "azurerm" {
  features {}
}

module "companynet" {
  source = "./modules/companynet"

  tenant_id         = var.tenant_id
  environment       = var.environment
  resource_groups   = var.resource_groups
  key_vaults        = var.key_vaults
  storage_accounts  = var.storage_accounts
  app_service_plans = var.app_service_plans
}

# modules/companynet/main.tf

module "resource_group" {
  source          = "../companynet.resource_group"
  environment     = var.environment
  resource_groups = var.resource_groups
}

module "key_vault" {
 source          = "../companynet.key_vault"
 tenant_id       = var.tenant_id
 environment     = var.environment
 resource_groups = "${module.resource_group.resource_groups.companynet}"
 key_vaults      = var.key_vaults

}

The module resource_group has the following main.tf:
# modules/companynet.resource_group/main.tf

resource "azurecaf_name" "resource_group" {
  for_each      = var.resource_groups
  name          = each.value.name
  resource_type = "azurerm_resource_group"
  suffixes      = ["${var.environment}", "001"]
}

resource "azurerm_resource_group" "resource_group" {
  for_each = var.resource_groups
  name     = azurecaf_name.resource_group[each.key].result
  location = each.value.location

}

but I don't know how to get the output of that resource_group name.
I have tried a few different things that do not work
# modules/companynet.resource_group/outputs.tf

output "resource_groups" {
 value = azurerm_resource_group.resource_group[*].name
}

value = azurerm_resource_group.resource_group.name
value = azurerm_resource_group.resource_group.companynet.name
value = azurerm_resource_group.resource_group[companynet].name
Each of these results in one error or another, all indicating a problem with modules/companynet.resource_group/outputs.tf
Ideally I would get an object that I can then iterate through in another module.  I expect to be able to call something like to get access to those resource group names in other modules such as:
# modules/companynet.key_vault/main.tf

resource "azurerm_key_vault" "key_vault" {
  for_each            = var.key_vaults
  name                = azurecaf_name.key_vault[each.key].result
  location            = var.resource_groups.location

  resource_groups     = "${module.resource_group.resource_groups.[companynet]}"

  sku_name            = "standard"
  tenant_id           = var.tenant_id
}

A: azurerm_resource_group.resource_group is declared with for_each, and so that expression refers to a map of objects where the keys match the keys of the for_each expression and the values are the corresponding declared resource instances.
In References to Resource Attributes there are various examples of referring to resource attributes in different situations, including the following about resources using for_each:

When a resource has the for_each argument set, the resource itself becomes a map of instance objects rather than a single object, and attributes of instances must be specified by key, or can be accessed using a for expression.

*

*aws_instance.example["a"].id returns the id of the "a"-keyed resource.

*[for value in aws_instance.example: value.id] returns a list of all of the ids of each of the instances.

That second item shows how to use a for expression to produce a list of the ids of aws_instance.example, but it doesn't show exactly how to produce a map and instead expects you to refer to the linked documentation about for expressions to learn about that:

The type of brackets around the for expression decide what type of result it produces.
The above example uses [ and ], which produces a tuple. If you use { and } instead, the result is an object and you must provide two result expressions that are separated by the => symbol:
{for s in var.list : s => upper(s)}

This expression produces an object whose attributes are the original elements from var.list and their corresponding values are the uppercase versions. For example, the resulting value might be as follows:
{
  foo = "FOO"
  bar = "BAR"
  baz = "BAZ"
}

A for expression alone can only produce either an object value or a tuple value, but Terraform's automatic type conversion rules mean that you can typically use the results in locations where lists, maps, and sets are expected.

This section describes how to produce an object and then notes that you can use the result in a location where a map is expected. In practice it's often possible to use object-typed values and mapped-type values interchangeably in Terraform, because they both have in common that they have elements identified by string keys. The difference is that an object type can have a separate type for each of its attributes, whereas a map must have the same type for all attributes.
Given all of this information, we can produce an object value describing the names for each resource group like this:
output "resource_groups" {
  value = { for k, g in azurerm_resource_group.resource_group : k => g.name }
}

For most purposes it doesn't really matter that this is an object-typed result rather than specifically a map, but since we know that .name is always a string we can infer that all of the attributes of this object have string-typed values, and so it would also be valid to explicitly convert to a map of strings using the tomap function (which is a "location where [...] maps [...] are expected", per the above documentation):
output "resource_groups" {
  value = tomap({
    for k, g in azurerm_resource_group.resource_group : k => g.name
  })
}

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