text:
\section{Introduction}

High degrees of deuterium fractionation in interstellar molecules have long been observed towards  star forming regions, in particular towards the cold and dense prestellar cores and envelopes of protostars. Indeed, because of the lower zero-point energy of H$_2$D$^+$ compared to that of H$_3^+$, the  deuterium exchange reaction  H$_3^+$ + HD $\rightarrow$ H$_2$ + H$_2$D$^+$ is slightly exothermic and favoured at temperatures lower than 20\,K, increasing the H$_2$D$^+$/H$_3^+$ ratio and therefore the possibility of transfering a deuterium atom to molecular species by ion-neutral chemistry. This ratio is further enhanced when CO, which is a major destroyer of the
H$_3^+$ ions, is frozen out on dust grains and undergoes a drastic abundance drop. In this case, the above-mentioned reaction becomes the  main reaction destroying H$_3^+$, which
leads to an increased H$_2$D$^+$/H$_3^+$  ratio, reaching  sometimes unity,  according to some models \citep{1992A&A...258..479P,2003ApJ...591L..41R}. Similar reactions with all deuterated isotopologues of H$_3^+$ also take place, leading to high abundances of H$_2$D$^+$, D$_2$H$^+$, and D$_3^+$ \citep{2003ApJ...591L..41R,2004A&A...418.1035W}.

Deuterium fractionation can theoretically be used to constrain molecular formation pathways, because the ratios between the deuterated species and the main isotopologue are expected to be different if the molecule forms in the gas phase or as a result of grain surface chemistry. In the latter case, deuteration is expected to follow a statistical scheme, as highlighted in, e.g, \citet{1989MNRAS.240P..25B}. The deuteration of such a ubiquitous molecule as ammonia has stimulated many studies, especially since the discovery of its triply deuterated isotopologue by \citet{2002ApJ...571L..55L} and \citet{2002A&A...388L..53V} with an abundance ratio ND$_3$/NH$_3\sim0.001$, an increase of 12 orders of magnitude with respect to the elemental D/H ratio \citep{2006ApJ...647.1106L}, challenging chemical models. As likely precursors of ammonia, nitrogen hydrides can bring valuable clues to constrain ammonia formation mechanisms. \citet{2015A&A...576A..99R} argue that highly-deuterated ammonia can form from pure gas phase chemistry. Observations of deuterated nitrogen hydride radicals like NHD and ND$_2$ can help to test this type of scenario.

The {\it Herschel Space observatory}\footnote{{\it Herschel} is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA} has allowed us to access the fundamental rotational transitions of nitrogen hydrides. Since its launch in 2009, both the NH radical and its deuterated counterpart have been detected towards the low-mass class 0 protostar IRAS16293-2422 \citep{2010A&A...521L..42B} and towards the dark core IRAS16293E \citep{2016A&A...587A..26B}. The abundances derived for these species have been found to be consistent with the model predictions of \citet{2005A&A...438..585R} and \citet{2015A&A...576A..99R}. The NH$_2$ radical has also been detected towards IRAS16293-2422 \citep{2010A&A...521L..52H} but no detection of its singly isotopologue NHD or doubly deuterated isotopologue ND$_2$
had been reported until recently.  However, while this manuscript was under revision, \citet{2020arXiv200707504M}  presented  the detection of the two latter species in IRAS16293-2422.

In this paper, we report the detection of both NHD and {\it para-}ND$_2$ towards IRAS16293-2422, based on different transitions from those in \citet{2020arXiv200707504M}, and discuss the implications of the derived abundances and abundance ratios on the formation of nitrogen hydrides. The observations are presented in Section\,\ref{obs}. In Section\,\ref{analysis}, we derive the abundances and discuss them in the light of new chemical models in Section \,\ref{mod}, before concluding in Section\,\ref{conclu}.

\section{Observations}
\label{obs}

The search for NHD and ND$_2$ was conducted towards IRAS16293-2422 which is a class 0 low-mass protostar where NH, ND and NH$_2$ had already been discovered \citep{2010A&A...521L..42B,2010A&A...521L..52H}. The coordinates of integration for the observations are $\alpha_{2000}=16^h$32$^m$22.8$^s$ $\delta_{2000}=-24{\degr}28^\prime33^{\prime\prime}$, the same as those where the  nitrogen hydrides were previously detected. While the source is a binary (composed of two sources A and B) \citep[see][for an extensive description of the source]{2016A&A...595A.117J}, the separation between the components is 5.1$\arcsec$, so that our observations encompass both components. The species NH, ND and NH$_2$ were all seen in absorption against a background emitted by the warm dust. This is partly due to the very high critical densities of the fundamental rotational transitions of nitrogen hydrides, especially NH$_2$ and NH \citep[around 10$^{7}$\,cm$^{-3}$, see][for the derivation of the collisional rate coefficients]{2012JChPh.137k4306D,2019MNRAS.tmp.2223B}, and the presence of the species in the lower density envelope. Indeed, the frequency of the fundamental rotational transition of ND is a factor of 2 smaller than for NH, and therefore the critical density a factor of $\sim 10$ smaller, making ND easier to be seen in emission than its hydrogenated counterpart.

\subsection{Spectroscopy}

Microwave spectroscopy measurements and analysis of NHD  have been performed by \citet{1997JChPh.107.9289K} and \citet{2013mss..confETH01M}, while those for ND$_2$ have been performed by \citet{1991JChPh..94.3423K} and \citet{2017ApJS..233...15M}. The spectra of both radicals have a complex fine and  hyperfine structure due to the interaction with the electronic and nuclear spins of nitrogen, deuterium and hydrogen (the latter only for NHD). For NHD, we targetted the group of hyperfine components ($N_{K_\mathrm{a} K_\mathrm{c}} J: 1_{0 1}\, 3/2 - 0_{0 0}\, 1/2$)\ around 412.7\,GHz. The $N_{K_\mathrm{a} K_\mathrm{c}} J: 1_{0 1}\, 1/2 - 0_{0 0}\, 1/2$ transition at 413.5\,GHz was additionally present in our observing bandwidth. For ND$_2$, the transitions ($N_{K_\mathrm{a} K_\mathrm{c}} J: 1_{1 1}\, 1/2 - 0_{0 0}\, 1/2$) at 531\,GHz were observed, which correspond to {\it para}-ND$_2$. The frequencies of the transitions and their Einstein coefficients for spontaneous emission are given in Table\,\ref{spectro_nhd1} and \ref{spectro_nhd2} for NHD and in Table\,\ref{spectro_nd2} for ND$_2$.

\subsection{NHD observations}

Singly deuterated amidogen was searched for with the APEX telescope\footnote{This publication is based on data acquired with the Atacama Pathfinder Experiment (APEX). APEX is a collaboration between the Max-Planck-Institut fur Radioastronomie, the European Southern Observatory, and the Onsala Space Observatory.}
on Chajnantor Plateau, Chile.
The observations were carried out in April 2013 in service mode with the Swedish heterodyne receiver instrument
APEX-3 \citep{2008A&A...490.1157V} tuned to 413.1\,GHz in the upper sideband. The receiver was connected to the XFFTS spectrometer
covering the entire receiver band with a spectral resolution of 0.076 kHz, corresponding to a velocity resolution of
0.055\,km\;s$^{-1}$ at this frequency.

During the observing runs, the amount of precipitable
water vapor was mostly between 0.8\,mm and 1.2\,mm, resulting in system temperatures between 400 and 500\,K
depending on source elevation. Because the NHD signal is expected to be moderately extended, the position
switching mode was used with an offset of 70\arcsec\ in Right Ascension to the West of the source, in a direction where the density
of the protostellar envelope and the molecular emission drops quickly \citep{2001A&A...375...40C}. The data were reduced
using the Gildas/CLASS software\footnote{http://www.iram.fr/IRAMFR/GILDAS}: the spectra were averaged together and a low
order polynomial was fitted to line-free regions of the spectra and subtracted.
The forward efficiency of the antenna was taken to be 0.95 and the beam efficiency 0.65, an intermediate value between
the measured value at 352\,GHz and that measured at 464\,GHz \citep{2006A&A...454L..13G}. These efficiencies were
used to convert the spectra from the $T_a^*$ to the $T_{\rm mb}$ scale. The APEX beam size is 15\arcsec\ full width at
half maximum (FWHM) at the observing frequency. The {\sl rms} noise in the spectrum is $\sim$\;33\,mK ($T_{\rm mb}$ scale)
in 0.11\,km\,s$^{-1}$ channels.

\subsection{ND$_2$ observations}
The search for doubly deuterated amidogen was carried out with the {\it Herschel}  Space Observatory \citep{2010A&A...518L...1P} in
the course of an open time project (PI: P. Hily-Blant, OBSID 1342227404). The ND$_2$ $N_{K_\mathrm{a} K_\mathrm{c}} J: 1_{1 1}\, 1/2 - 0_{0 0}\, 1/2$ line at 531\,GHz was observed with the HIFI instrument \citep{2010A&A...518L...6D} in band 1a
on 26 August 2011 (OBSIDs 1342227403 and 1342227404), with both the wide band spectrometer (WBS), and the high resolution spectrometer (HRS). The WBS has a spectral resolution of 1.1\,MHz, corresponding to a velocity resolution of 0.6\,km\,s$^{-1}$ at the frequency of the observations, and the HRS has a resolution of 0.25\,MHz, corresponding
to a velocity resolution of 0.14\,km\,s$^{-1}$. The observations were performed in the single pointing dual beam switch mode with fast chopping (4\,Hz)
and optimization of the continuum. This improves the subtraction of the standing waves and the determination of the continuum. In
this mode, the OFF positions are at fixed offsets 3$\arcmin$ away from the source coordinates on either side (East-West) of the source. We checked on the spectra
of these OFF positions that no ND$_2$ signal was present. The data were processed with the HIPE pipeline \citep{2010ASPC..434..139O} version 14 up to level\,2.5 products, after which they were exported to Gildas/CLASS data format for further analysis: the spectra in both horizontal and vertical polarizations were averaged, and a first order polynomial baseline  was fitted to line-free regions of the spectrum and subtracted.  The HIFI beam at 531\,GHz, the frequency of the ND$_2$ transitions, is $\sim 39$\arcsec\ FWHM, the main beam efficiency $\eta_\mathrm{mb}$ is 0.62 and the forward efficiency $\eta_\mathrm{fwd}$ is 0.96  \citep{2017A&A...608A..49S}. The {\sl rms} noise in the spectrum is $\sim$\;6.6\,mK ($T_{\rm mb}$ scale) in 0.56\,km\,s$^{-1}$ channels.

\subsection{Continuum data}

In this study, we also used continuum data (see section\,\ref{continuum}).  Maps at 250\,$\mu$m, 350\,$\mu$m, and 500\,$\mu$m
observed by  {\it Herschel}/SPIRE \citep{2010A&A...518L...3G} were taken from the {\it Herschel} Gould Belt survey  \citep[HGBS][]{2010A&A...518L.102A}.
We used the level 2.5 maps of the L1689 cloud (OBSID 1342239773)  processed by the HIPE pipeline (version 12.0) and calibrated for extended sources. Absolute calibration  using HFI data from the Planck satellite is also performed by the pipeline. We also subtracted from the images a constant offset measured in an apparently emission-free region to the South-East of the L1689 cloud. This serves as a first-order removal of the emission from the diffuse galactic background.  Because the {\it Herschel}/SPIRE maps focus on a $\sim 15\arcmin\times 15$\arcmin region centered on IRAS16293-2422 and do not include areas outside of the Rho Ophiuchi cloud, we used the larger-scale maps of Rho Ophiuchi covering the whole complex (OBSID 1342205093 and 1342205094, also part of the HGBS) to measure the off-cloud emission for each of the three wavelengths. These values were corrected from the intensity offsets between the small maps of IRAS16293-2422 and the large-scale maps of Rho Ophiuchi by comparing the map intensities in a region common to both types of maps.

The beam sizes (FWHM) at wavelengths 250, 350, and 500\,$\mu$m are 18\arcsec, 25\arcsec and 36\arcsec, respectively. As in \citet{2016A&A...587A..26B}, additional ground-based maps of the region at 850\,$\mu$m taken with the  SCUBA-2 bolometer array on the {\it James Clark Maxwell telescope} (JCMT) as part of the JCMT Gould Belt Survey \citep{2013MNRAS.430.2513H}  were used. The data and the data reduction procedure are described in \citet{2015MNRAS.450.1094P}. Finally, we also used the map at 1.2\,mm taken by  \citet{2002ApJ...569..322L} with the MAMBO-II bolometer on IRAM\,30m telescope. The FWHM beamsizes are $\sim 14$\arcsec\ for the JCMT/SCUBA-2 map and $\sim 11$\arcsec\ for the IRAM 30\,m data.

\section{Results and analysis}
\label{analysis}

\subsection{Continuum estimation\label{continuum}}

\subsubsection{NHD}

Because the ground-based observations do not enable us to measure the continuum level of the NHD spectrum, we use available
continuum observations taken at various wavelengths to infer the value at the frequency of the NHD transition (413\,GHz, which corresponds
to a wavelength of 726\,$\mu$m) by interpolation.  At wavelengths larger than typically 200\,$\mu$m, the spectral energy distribution of the protostar is close to the Rayleigh-Jeans regime, so that fitting a simple power-law to the source fluxes as a function of wavelength allows for a straightforward determination of the continuum value
at 413\,GHz. First the continuum maps were smoothed to a common angular resolution, i.e. 36$\arcsec$,  that of the coarsest map from SPIRE at 500$\mu$m. To achieve this, the 250\,$\mu$m, 350\,$\mu$m and 500\,$\mu$m SPIRE maps were convolved with the appropriate kernels provided by \citet{2011PASP..123.1218A}. The 850$\mu$m SCUBA-2 map and the 1.2\,mm MAMBO-II map were convolved with gaussian kernels of FWHM 33\,$\arcsec$ and 34.3$\arcsec$, respectively, the former also from \citet{2011PASP..123.1218A}. The average surface brightnesses of the source at each wavelength were measured in an aperture of 15$\arcsec$, corresponding to the beam of the NHD observations. We also added the continuum intensity from the {\it Herschel}/HIFI ND$_2$ spectrum at 531\,GHz (565$\mu$m), which is at a similar resolution. A power-law of index $\alpha=-2.6$ could be fitted to the data points (Fig.\,\ref{sed}), which enabled us to interpolate the intensity at 413\,GHz at a resolution of 36$\arcsec$. To derive the source intensity at the resolution of the APEX observations (15$\arcsec$), we smoothed the SCUBA-2 map to the resolution of the APEX observations by convolution with a gaussian kernel of 5$\arcsec$ from \citet{2011PASP..123.1218A}, and the MAMBO-II bolometer map by convolution with a gaussian kernel of 10.2$\arcsec$ FWHM. Those two points were fitted with a power-law with the same exponent $\alpha$, and from this power-law, the value of the surface brightness was obtained at 413\,GHz at a resolution of 15$\arcsec$. This method assumes that the dust opacity index does not depend on the angular resolution, i.e. on the dust temperature or density in the ranges probed by the observations. While this might not be true in the general case, this approximation is good enough for our purpose here, considering the uncertainties in the data analysis. The interpolated surface brightness is 3154\,MJy/sr, corresponding to a brightness temperature $T_c (\mathrm{NHD})=600$\,mK. We used the latter value as the continuum brightness temperature of the source in the APEX spectrum.

Because of the observing technique used to remove the strong atmospheric emission for ground-based observations, the emission arising from extended structures in the astrophysical source is partly filtered out.  Since we are interested in the mean intensity of the protostar in a compact region around its maximum, our surface brightness values at 850\,$\mu$m and 1.2\,mm should not be too affected. Nevertheless, the filtering of the extended emission for the JCMT and IRAM 30\,m maps could lead to an underestimate of the surface brightness at 850\,$\mu$m and 1.2\,mm. Therefore, the power-law that we fitted could in fact be shallower and the continuum intensity at 413\,GHz could be slightly overestimated.

 \begin{figure}
  \centering
  \includegraphics[width=8cm]{continuum.eps}

  \caption{Continuum intensities of IRAS16293-2422 measured at 36$\arcsec$ resolution (red dots) and power-law fit (red dashed line). The index of the power-law is found to be $\alpha=-2.6$. The blue squares are the intensities at
  15$\arcsec$ resolution, and the blue dash-dotted line fits these points with the same power-law index $\alpha$. The derived intensity $I_0$  at the wavelength of the APEX observations ($\lambda_0=726\,\mu$m) and at a resolution of 15$\arcsec$ is marked as a blue diamond.}
             \label{sed}%
  \end{figure}

\subsubsection{ND$_2$}

For ND$_2$, the continuum was measured by fitting a zeroth order polynomial to the spectrum
in regions that do not show any spectral lines. Assuming that the observed continuum is the sum of that in the upper side-band and that in the lower side-band, and supposing that it increases with frequency following a power-law of index $\alpha=-2.6$, we find that the single side band continuum at 531\,GHz is $T_c (\mathrm{ND_2})=210$\,mK.

\subsection{NHD and ND$_2$ spectra}

The observed NHD and para-ND$_2$ spectra are shown in Fig.\,\ref{nhdnd2}. For both spectra, the continuum levels derived in section\,\ref{continuum} were added to the spectra after baseline withdrawal. Both molecules are seen in absorption against the continuum. For the NHD spectrum, a rather broad emission feature (rest frequency 412702.5\,MHz) is visible at a similar velocity as that of the NHD lines. The FWHM of this feature is $\sim$\,8.5\,km s$^{-1}$, like for other similarly-looking features in the spectrum. Such wide spectral lines have already been seen  in this source \citep[e.g. TIMASSS,][]{2011A&A...532A..23C}, and are consistent with that of lines emitted in the hotter central region. However these broad emission lines unlikely arise from NHD itself: the near-gaussian feature against which the two strongest NHD features are seen in absorption peaks at a velocity $\sim$ 6.5\,km\,s$^{-1}$, higher than the hot corino velocity at 3.1\,km\,s$^{-1}$ and 2.7\,km\,s$^{-1}$ for sources A and B, respectively \citep{2011A&A...534A.100J,2016A&A...595A.117J}, and than the line velocities measured in the TIMASSS survey  (lower than 5\,km\,s$^{-1}$). In the following, we have considered that this feature arises from an unknown molecular transition (different from NHD), but we cannot fully exclude the possibility that it is a baseline ripple. The other strong, broad emission lines seen in Fig.\,\ref{nhdfit} (e.g., at  412738.7\,MHz, 413541.1\,MHz, and 413564.9\,MHz) are also unidentified and probably arise from the warm inner region.

 \begin{figure}
   \centering
   \includegraphics[width=8cm]{fig_spectra.eps}

   \caption{NHD (bottom panel) and ND$_2$ (top panel) spectra in IRAS16293-2422. The red sketch shows the positions and expected relative
   intensities of the hyperfine components. The strong emission feature at a velocity of $-$10\,km s$^{-1}$ (corresponding to a frequency of 531079.2\,MHz)
   in the ND$_2$ spectrum is likely the $N_{K_\mathrm{a} K_\mathrm{c}}: 11_{1\;11}-10_{1\,10}$ transition of CH$_3$OH. The broad features in the NHD spectrum at velocities $-17$\,km\,s$^{-1}$ and
   7\,km\,s$^{-1}$ are unidentified.}
              \label{nhdnd2}%
    \end{figure}

Several hyperfine components are detected with the expected velocity shifts both for NHD ($J$: 3/2 $-$ 1/2) at 412.7\,GHz and para-ND$_2$ at 531\,GHz. No hyperfine component is seen for the NHD $J$: 1/2 $-$ 1/2 transition at 413.5\,GHz (Fig.\,\ref{nhdfit}). The source velocity is found to be 4.1\,km\;s$^{-1}$ for both NHD and ND$_2$. This is about 0.3\;km\;s$^{-1}$ higher than the velocities of 3.8\,km\;s$^{-1}$ for ND, NH and NH$_2$ in the same source \citep{2010A&A...521L..42B,2010A&A...521L..52H}, hinting at possibly different spatial locations for the deuterated forms of amidogen, or a lack of accuracy in the values of the rest frequencies. Because the noise in the spectra is relatively high, only the hyperfine components that are expected to be the strongest are detected, and no  theoretically weak component is detected, so that we are confident that both species are present.

The fact that the lines are seen in absorption and their narrow linewidths ($\Delta v = 0.5$\,km\;s$^{-1}$ for NHD and $\Delta v\sim 0.7$\,km\;s$^{-1}$ for ND$_2$, though the latter value is subject to more uncertainty because of the lower signal-to-noise ratio) is consistent with the presence of both species in the low-density and low-temperature protostellar envelope, rather than in the higher density regions close to the hot core.

\subsection{Column density estimates}

Both NHD and ND$_2$ spectra were analysed in a similar fashion: the optical depth was derived as a function of frequency given a column density and assuming the same excitation temperature for all the hyperfine components. Because of the overlap between the hyperfine components, such a simple model may not be able to reproduce well the line relative ratios. More sophisticated and accurate treatments are not possible, since collisional coefficients are not yet available for these two species. The consequence on the column density determination should remain limited because of the low optical depths of the transitions. For Gaussian lines, the velocity integrated optical depth  is
\begin{equation*}
\int{\tau(v) dv} = \tau_0 \Delta v \sqrt{\frac{\pi}{4\ln{(2)}}}
\end{equation*}
where $\tau_0$ is the line central optical depth and $\Delta v$ the line full width at half maximum.
The optical depth at line centre is therefore given by\\
\begin{equation*}
\tau_0 = N \frac{c^3}{8\pi\nu^3 }\frac{A_\mathrm{ul} g_\mathrm{up} }{Q(T_\mathrm{ex})}\frac{e^{h\nu/(k_\mathrm{b}T_\mathrm{ex})}-1}{e^{E_\mathrm{up}/k_\mathrm{b}T_\mathrm{ex}}}\frac{1}{\Delta v}\sqrt{\frac{4\ln{(2)}}{\pi}}
\end{equation*}
where $Q(T_\mathrm{ex})$ is the partition function at excitation temperature $T_\mathrm{ex}$, $N$ is the total molecular column density, $\nu$ the frequency of the transition, $A_\mathrm{ul}$ the Einstein spontaneous emission coefficient of the transition, $g_\mathrm{up}$ the upper level degeneracy, $c$ the speed of light, $E_\mathrm{up}$ the energy of the upper level, and $h$ and $k_\mathrm{b}$ are the Planck and Boltzmann constants, respectively. The total optical depth as a function of velocity is given by (neglecting the effect of line overlap on line excitation)\\
\begin{equation*}
\tau(v) = \sum_i \tau_0^i \exp{\left(-4\ln{(2)}\left(\frac{v-v_0}{\Delta v}\right)^2\right)}
\end{equation*}
where $v_0$ is the rest velocity, $i$ refers to hyperfine component $i$ and $\tau_0^i$ the optical depth of the hyperfine component $i$ is  $\tau_0^i=\tau_0 R_i$, with $R_i$ the hyperfine component statistical weight.
The brightness temperature is then simply \\
\begin{equation*}
T_\mathrm{b}(v) = (J_\nu(T_\mathrm{ex})-J_\nu(T_\mathrm{CMB}))(1-e^{-\tau(v)})+ T_\mathrm{c}\ e^{-\tau(v)}
\end{equation*}
with $J_\nu(T)$ the Rayleigh-Jeans equivalent temperature, $T_\mathrm{CMB}$ the temperature of the cosmic microwave background ($T_\mathrm{CMB} = 2.73$\,K) and $T_\mathrm{c}$ the continuum temperature ($T_\mathrm{c} = 600$\,mK for NHD and $T_\mathrm{c} = 210$\,mK for ND$_2$, see Section\,\ref{continuum}).

The observed spectra were then fitted by adjusting the value of the column density, having assumed an excitation temperature. We assumed an excitation temperature of 3\,K, but the influence on the column density value is basically unchanged for an excitation temperature range of $2.8-4$\,K. This is a reasonable assumption for lines seen in absorption, however from our spectra we cannot fully exclude higher values of $T_\mathrm{ex}$, which would lead to the need for higher column densities to fit the spectra. For excitation temperatures larger than 5.3\,K for ND$_2$ and 5.8\,K for NHD, the lines would be seen in emission. For NHD, we assumed that the line is seen in absorption against a background varying with velocity and made of the dust continuum and a line possibly originating from the hot core with a FWHM linewidth of 8.5\,km\,s$^{-1}$.

With $T_\mathrm{ex} = 3$\,K, we find column densities of $N \sim  3.9\times 10^{13}$\,cm$^{-2}$ for NHD and  $N \sim 7\times 10^{12}$\,cm$^{-2}$ for para-ND$_2$. For these column density values, the maximum optical depth is 0.5 for the components of NHD and 0.3 for those of ND$_2$. Assuming
 an ortho-to-para ratio of 0.4 for ND$_2$, consistent with the ortho-to-para ratio derived from the observations of \citet{2020arXiv200707504M},  we find that the total (ortho+para) ND$_2$ column density is $\sim  10^{13}$ cm$^{-2}$. Note that in the case of NH$_2$ the excitation temperature could be determined from the relative ratios of the hyperfine components because of the high signal-to-noise ratio of the spectra, and was found to be $\sim$\,9\,K \citep{2010A&A...521L..52H}.

We note that the critical densities associated with the detected transitions are $\gtrsim 10^6$~cm$^{-3}$ assuming collisional rate coefficients for NHD and ND$_2$ of a few 10$^{-11}$~cm$^3$s$^{-1}$ \citep[see][for the main isotopologue NH$_2$]{2019MNRAS.tmp.2223B}. Excitation temperatures are therefore expected to be lower than the kinetic temperature in the protostellar envelope where $T_\mathrm{kin}\sim 10$~K and $n \sim 10^5$~cm$^{-3}$, but will depend on the exact physical conditions of the absorbing molecules.

Acceptable fits are found for $N\mathrm{(NHD)} \sim 3.2 \times 10^{13} - 4.7\times 10^{13}$\,cm$^{-2}$ and we adopt this range for the uncertainty on the NHD column density value. Uncertainties on the para-ND$_2$ column density value are $\sim 5\times 10^{12} - 8\times 10^{12}$\,cm$^{-2}$. The fits are shown in Fig.\,\ref{nhdfit} and Fig.\,\ref{nd2fit} for NHD and ND$_2$, respectively.

   \begin{figure*}

  \centering
            \includegraphics[width=18cm]{nhd_fit_all.eps}
      \caption{NHD spectra for the J: 3/2-1/2 (left panel) and J: 1/2-1/2 (right panel) transitions (blue line) and model spectra (red line). The broad emission features at 412702.5\,MHz, 412738.7\,MHz, 413541.1\,MHz, and 413564.9\,MHz, are unidentified molecular lines probably originating in the warm inner regions.}
         \label{nhdfit}
   \end{figure*}

   \begin{figure}

  \centering
            \includegraphics[width=9cm]{nd2_fit.eps}
      \caption{ND$_2$ spectrum for the J: 1/2-1/2 transition (blue line) and model spectrum (red line). }
         \label{nd2fit}
   \end{figure}

As mentioned before, we cannot exclude that the signal against which the NHD transitions are seen is due to atmospheric fluctuations (i.e. foreground emission). Assuming this is the case, we first withdrew a high-order (e.g. 9) polynomial to the spectrum, excluding only the NHD absorption features from the fit, after which we proceeded with fitting the spectrum as described above. In this case, and assuming an excitation temperature of $T_{\rm ex}=3\,$K as well, the NHD column density needed to fit the absorption feature is $N\sim 4.6\times 10^{13}$\,cm$^{-2}$. This is within the uncertainties of our previous NHD column density determination.

Table\,\ref{coldens} sums up the observed column densities  for ortho-NH$_2$, NHD and para-ND$_2$. These values are consistent with the ones derived by \citet{2020arXiv200707504M}. Note that for the designation of spin symmetries, we have followed the standard Maue's rule \citep{1937AnP...422..555M} where the ortho species have the largest statistical weight and para species have the smallest statistical weight. Thus, in the case of ND$_2$, the symmetric rotational levels (K$_a$+K$_c$ even) combine with antisymmetric nuclear spin function I$_D$=1 i.e. para states, while antisymmetric rotational levels (K$_a$+K$_c$ odd) combine with symmetric nuclear spin function I$_D$=0, 2 i.e. ortho states. The reverse convention was employed in \citet[][see their Appendix A.2]{2020arXiv200707504M}, hence our value of column density for para-ND$_2$ should be compared with their value for ortho-ND$_2$.

\subsection{Abundance ratios}

\citet{2010A&A...521L..52H} observed ortho-NH$_2$ at the same position in IRAS16293-2422. Based on this observation, and assuming an ortho-to-para ratio of 2, close to the value suggested by their model, \citet{2014A&A...562A..83L}  derived a total (ortho+para) NH$_2$ column density of $7.5\times 10^{13}$ cm$^{-2}$, which we adopt here. This leads to relative column density ratios NH$_2$:NHD:ND$_2$ of $\sim$  8:4:1.

Large ratios between singly deuterated molecules and main isotopologues of a few 10\% such as we find here for NHD/NH$_2$ are common in protostellar envelopes, for molecules formed in the later stages of prestellar evolution \citep[e.g. formaldehyde, methanol, or ammonia, but unlike water, see ][]{2013A&A...550A.127T}, although the case of the amidogen radical presented here is rather extreme. For example in IRAS16293-2422, HDCO/H$_2$CO is $13-16$\% \citep{2000A&A...359.1169L}, CH$_2$DOH/CH$_3$OH is $10-50$\% \citep{2004A&A...416..159P} and NH$_2$D/NH$_3$ is 10\% \citep{1995ApJ...447..760V}. For ammonia, \citet{2005A&A...438..585R} have compiled NH$_2$D/NH$_3$ ratios between 10\% and 30\% in a sample of sources made of dense cores and protostars. Such fractionation ratios can usually be accounted for by present chemical models \citep[e.g.][]{2012ApJ...760...40A,2015A&A...576A..99R}.

The high abundance of ND$_2$  is reminiscent of other molecules, for which
 it has been observed that doubly deuterated species were often overabundant. Indeed, the ratio between the doubly- and the singly-deuterated isotopomers is in some  species even larger than the ratio between the singly deuterated  and the main isotopologue. In IRAS16293-2422, D$_2$CO/HDCO is 30$-$40\% \citep{2000A&A...359.1169L}, i.e. $2-3$ times higher than HDCO/H$_2$CO. Other protostellar envelopes are also characterised by D$_2$CO/HDCO ratios which are higher than HDCO/H$_2$CO ratios \citep{2006A&A...453..949P} \citep[see also the D$_2$CO/HDCO measurement in the cloud $\rho$ Oph A by][]{2011A&A...527A..39B}. For ammonia and methanol, the ratios XD$_2$/XHD (where X represents the species) are of the same order (though slightly lower) as the XHD/XH$_2$ ratios \citep{2006A&A...453..949P,2005A&A...438..585R}.  Water is also characterised by high abundances of its doubly deuterated isotopologue, with D$_2$O/HDO > HDO/H$_2$O in the envelope of IRAS16293-2422, as reported by \citet{2013A&A...553A..75C}. Moreover, high angular resolution interferometric observations sampling the warm inner regions of young protostars show very high abundances of doubly deuterated molecules: in NGC1333-IRAS2, D$_2$O/HDO is found to be seven times higher than HDO/H$_2$O \citep{2014ApJ...792L...5C}. Other species like formaldehyde, observed with ALMA in the hot core of IRAS16293-2422 \citep{2018A&A...610A..54P} or doubly deuterated methyl formate, which was recently detected in the hot core of IRAS16293-2422 \citep{2019A&A...623A..69M}  similarly show XD$_2$/XHD ratios typically $2-3$ times higher than the XHD/XH$_2$ ratio. So far, chemical models have struggled to explain this feature.

\section{Chemical model}
\label{mod}

We compare the observed column densities with the predictions of the gas-grain chemical model presented in \citet{2018MNRAS.477.4454H}. The model is based on the University of Grenoble Astrochemical Network (UGAN), which includes the nuclear-spin states of H$_2$, H$_2^+$, H$_3^+$ and of all the carbon, nitrogen, oxygen and sulfur containing hydrides,
as well as their abundant deuterated forms. Grain-surface reactions are not explicitly included in the UGAN network, except the formation (and immediate desorption) of H$_2$ and isotopologues. The rates of adsorption and desorption and the list of species assumed to form in grain mantes can be found in \citet{2018MNRAS.477.4454H}. In this model, nitrogen hydrides are formed exclusively by gas-phase reactions.
An update of the oxygen hydrides chemistry was recently performed by \citet{2019MNRAS.487.3392F}. The dynamical model is presented in \citet{2018MNRAS.477.4454H} and is inspired from the studies of gravitational collapse by \citet{1969MNRAS.145..271L} and \citet{1969MNRAS.144..425P}. Briefly,
the core, which is considered to have a constant density central plateau surrounded by an enveloppe of density falling as $r^{-2}$, where $r$ is the radius, collapses self similarly.

The density of the central plateau is homogeneous and increases with time while its contribution to the total mass and total radius (and therefore total column density) decreases with time. Full details can be found in \citet{2018MNRAS.477.4454H}. The model was run for  a kinetic temperature fixed at $T=10$~K and an initial core density $n_{\rm H}=10^4$~cm$^{-3}$. Other parameters can be found in Table~1 of \citet[][`reference` model]{2018MNRAS.477.4454H}.

The total column density for ortho-NH$_2$, NHD and para-ND$_2$, and the contribution of the envelope, are shown as a function of the core density in Fig.\,\ref{modelfigure}, where the observational error bars include the uncertainty on the excitation temperatures. As may be seen, the contribution of the central plateau to the total column density reaches a maximum at a central density $n_{\rm H}\approx 3-6\times 10^6$\,cm$^{-3}$, and is then negligible above typically $5\times 10^7$\,cm$^{-3}$. Incidentally, at an evolution time of the cloud corresponding to a central density of $n_{\rm H}\approx 6.5\times10^{6}$~cm$^{-3}$, the column densities of the envelope derived from the model are $2.7\times 10^{13}$ and $2.5\times 10^{13}$\,cm$^{-2}$, for ortho-NH$_2$ and NHD, respectively. Although the model agrees with the observational constraints at this stage of cloud evolution, very good agreement is obtained also at central densities above 10$^7$\,cm$^{-3}$, while the contribution of the plateau is already mitigated. For para-ND$_2$, on the other hand, the total (core + envelope) column density matches the observation values at $n_\mathrm{H}=6.5\times 10^6$\,cm$^{-3}$. At larger core densities (where the envelope dominates) the model underestimates the observational value by a factor of $\sim 2-3$. It may be emphasised that, on observational grounds, the detected molecules most likely belong to the envelope for at least two reasons: lines are seen in absorption, and also, because the diameter of the inner plateau is $10^3$\,au, or 7\arcsec\ \citep[at a distance of 140\,pc $-$][]{2018A&A...614A..20D} when $n_{\rm H}$ reaches $6.5\times 10^5$\,cm$^{-3}$. As a result, while our model can reproduce the column density of ortho-NH$_2$ and NHD within a factor of 2, it is found to underestimate that of para-ND$_2$ by a factor larger than 2. At a central density of 10$^7$\,cm$^{-3}$, the abundance ratios are 8.7:6.4:1 for NH$_2$:NHD:ND$_2$, with ortho-NH$_2$/para-NH$_2$=1.9 and ortho-ND$_2$/para-ND$_2$=3.1. We also note that the ortho-to-para ratio of NH$_2$ stays very close to 2 throughout the collapse, while that of ND$_2$ increases steadily from 2.1 to 3.1. While the above successive deuteration ratios taking into account the total (ortho+para) column densities of NH$_2$ and ND$_2$ agree with our observations to within a factor of two (see Table\,\ref{coldens}), our model has trouble reproducing such a low ortho-to-para ratio of ND$_2$ as found by \citet{2020arXiv200707504M}. This possibly suggests that some thermalisation reactions are missing in our UGAN network, since the measured ortho-to-para ratio corresponds to a spin temperature as low as $5-6$\,K\footnote{We note that at temperatures below $\sim$ 10\,K, the ortho-to-para ratio of ND$_2$ can be approximated by the function $6\times\exp{(-15.5/T_\mathrm{spin})}$}. Finally, our model predicts that the NH$_2$:NHD:ND$_2$ ratios remain constant and equal to 7.1:5.6:1 above a density of $3\times 10^7$ cm$^{-3}$.

These results indicate that pure gas-phase chemistry as in the UGAN model can reproduce the observed column densities and abundance ratios of the amidogen radical isotopologues in protostellar envelopes within a factor of $\sim$\,2$-$3. We note, however, that we have assumed identical rate coefficients for dissociative recombination of all deuterated isotopologues of NH$_4^+$ with, in addition, statistical H/D branching ratios for the products. These assumptions are questionable because DR experiments have suggested the occurence of isotope effects \citep[e.g.][]{2004JChPh.120.7391O}. This will be investigated in a future, more complete, modelling study.

\begin{table}
	\center
	\caption{Comparison  between chemical model predictions at a central density of 10$^7$ cm$^{-3}$, and observational constraints for the column density of ortho-NH$_2$, NHD, and para-ND$_2$. The model values are for the envelope. Also given are the ortho-to-para ratios and total column densities for NH$_2$ and ND$_2$ as obtained with the UGAN model. The last column sums up the observational values from the work by \citet{2020arXiv200707504M}. \label{coldens}}
	\begin{tabular}{c c c c}

		Species & Model & Observation & \citet{2020arXiv200707504M} \\
		& & (this work) & \\
		& (cm$^{-2}$) & (cm$^{-2}$) & (cm$^{-2}$) \\
		\hline
		ortho-NH$_2$ &            $2.9\times 10^{13}$& $5.0\times 10^{13}$ & $5.4\times 10^{13}$\\
		para-NH$_2$ &            $1.5\times 10^{13}$\\
		NHD  &            $3.2\times 10^{13}$ & $3.9\times 10^{13}$ & $4.7\times 10^{13}$ \\
		ortho-ND$_2$ &            $3.8\times 10^{12}$ & & $2.4\times 10^{12}$ \\
		para-ND$_2$ &            $1.2\times 10^{12}$ & $7.0\times 10^{12}$ & $6.6\times 10^{12}$ \\
		NH$_2$  & $4.4\times 10^{13}$\\
		ND$_2$  & $5.0\times 10^{12}$ \\
		ortho-NH$_2$/para-NH$_2$ &     1.9\\
		ortho-ND$_2$/para-ND$_2$ &     3.1 & & 0.4\\
		NH$_2$/ND$_2$   &      8.7\\
		NHD/ND$_2$   &      6.4\\
		\hline
	\end{tabular}
\end{table}

Statistical distributions of deuterium atoms is expected if nitrogen hydrides form by successive hydrogenations of nitrogen atoms on grain surfaces \citep{1982A&A...114..245T,1989MNRAS.240P..25B,1997ApJ...482L.203C}.
According to the grain-surface addition scheme, NHD/NH$_2 = 2$\,D/H (where D/H denotes the {\it atomic} D over H ratio) and ND$_2$/NH$_2$= (D/H)$^2$. This leads to ND$_2$/NHD =  0.25 NHD/NH$_2$. This value is  consistent  with the observed ratios, for which ND$_2$/NHD = 1/2 NHD/NH$_2$ within a factor of two.
Therefore, although grain surface chemistry is not needed to account for the observed abundances of these species, we cannot exclude grain-surface processes either.
We note that the ortho-to-para ratios provide additional constraints but current measurements have large uncertainties \citep{2020arXiv200707504M,2017A&A...600A..61H,2018MNRAS.477.4454H}. Indeed, taking the ortho-to-para ratio for ND$_2$ as 3 as indicated by our chemical model in the late collapse stages, we find a total ND$_2$ column density of $4.8\times 10^{13}$\,cm$^{-2}$. This in turn leads to ND$_2$/NHD = 4/3 NHD/NH$_2$, with which the statistical grain-surface scenario is inconsistent.

Our analysis and chemical model are based on the hypothesis that all species are coexistent. However, in the case of NH and ND, a detailed radiative transfer model of the spectra of these two species seen towards the dense core IRAS16293E showed that the signal from NH and that from ND came from spatially separate regions \citep{2016A&A...587A..26B}, with the ND transition sampling higher density material.
It is possible as well that in the case of amidogen, the deuterated isotopologue is concentrated at higher densities than NH$_2$, and even more so for the doubly-deuterated isotopologue. Indeed deuteration proceeds faster at higher densities because it is tightly linked to the depletion of abundant gas-phase species like CO.
The discrepancy between the model and the ND$_2$ observations could also indicate that important fractionation reactions are missing from the model.

In order to assess the sensitivity of our results to the assumed  excitation temperature, we have derived the column densities assuming $T_{\rm ex}=4.5$\,K. With this value, we find $N$(NHD)$ = 7\times 10^{13}$\,cm$^{-2}$ and $N$(para-ND$_2) = 1.2\times 10^{13}$\,cm$^{-2}$, i.e. a total (ortho+para) column density of ND$_2$ $N$(ND$_2$) =  $1.7\times 10^{13}$\,cm$^{-2}$, assuming as before an ortho-to-para ratio of 0.4 for ND$_2$. While for NH$_2$, the excitation temperature could be determined by fitting the relative ratios of the hyperfine components \citep{2010A&A...521L..52H}, this is not possible for NHD and ND$_2$ because of the low signal-to-noise ratio of the observations. With these column density values, the relative ratios between the different amidogen isotopologues are  4 :  4 : 1 for NH$_2$ : NHD : ND$_2$. Clearly, a non-LTE model is required in order to derive more accurate column densities and abundance ratios. This will be performed in a forthcoming paper thanks to the next availability of collisional rate coefficients for NHD and ND$_2$ (Bop et al., in prep.)

\begin{figure}
\centering
\includegraphics[width=8cm,angle=0]{ugan_model_v3.png}
\caption{\label{modelfigure}Model predictions \citep{2018MNRAS.477.4454H} showing the predicted column densities of NH$_2$, NHD, and ND$_2$ as a function of core density (see text). The dashed lines represent the column density of the envelope, while the solid lines represent the total (core + envelope) column density. The shaded rectangles show the observed column densities.}
         \label{model}
  \end{figure}

\section{Conclusions}
\label{conclu}
We have detected the singly-deuterated  and doubly-deuterated isotopologues of amidogen, NHD and para-ND$_2$  towards the envelope of the class 0 protostar IRAS16293-2422. The column densities of NHD and  para-ND$_2$ are estimated to be $3.2 \times 10^{13} - 7\times 10^{13}$ cm$^{-2}$ and  $5\times 10^{12} - 1.2\times 10^{13}$ cm$^{-2}$, respectively. The
observed relative ratios between the deuterated isotopologues and the main isotopologue NH$_2$ can be reproduced within a factor of  $2-3$ with our pure gas-phase chemical model.
This result adds to previous evidence that pure gas-phase chemistry can reproduce many features
(i.e. spin-state ratios for NH$_2$, deuterium fractionation, abundances) observed in nitrogen hydrides \citep{2018MNRAS.477.4454H}. However, the data are also
consistent  with the statistical ratios expected from grain-surface chemistry. A more elaborate analysis of the observations is necessary taking into account the different angular resolutions for NHD and ND$_2$ as well as likely non-LTE excitation effects. A better understanding  of the ortho-to-para ratio in ND$_2$ might help to distinguish between both chemical routes.

\section*{Acknowledgements}
This research has made
use of data from the {\it Herschel} Gould Belt survey (HGBS) project (http://gouldbelt-herschel.cea.fr). The HGBS is a {\it Herschel} Key Programme jointly
carried out by SPIRE Specialist Astronomy Group 3 (SAG 3), scientists of several institutes in the PACS Consortium
(CEA Saclay, INAF-IFSI Rome and INAF-Arcetri, KU Leuven, MPIA Heidelberg), and scientists of the {\it Herschel} Science Center (HSC). This work has been supported by the Agence Nationale de la Recherche (ANR-HYDRIDES), contract ANR-12-BS05-0011-01. This work was supported by the Programme National "Physique et
Chimie du Milieu Interstellaire" (PCMI) of CNRS/INSU with INC/INP co-funded
by CEA and CNES.

\section*{Data Availability}

The data underlying this article were accessed from the ESO archive (APEX data) and The Herschel Space Observatory archive (HIFI/Herschel data)

\bibliographystyle{mnras}

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text:
In the Director's Chair: An Interview with Ivan Heng
Ivan Heng is pulling triple duty! What excites him as Co-Artistic Director of Singapore Theatre Festival 2018? And what it's like directing two brand-new plays – Tan Tarn How's Press Gang and Pam Oei's Faghag – at the same time?
Nice work if you can get it! Ivan's smile lights up the room during rehearsals for Faghag
This year's Singapore Theatre Festival features eight brand-new plays. What thrills you about the line-up?
The fact that every single play in this season is for and about Singapore. I founded WILD RICE because I felt that Singaporean stories need to be told. So it's especially thrilling to work on eight new and original works.
While each of these plays are told from a distinctly Singaporean point of view, each show also speaks to the universal experience of being human and the times we live in. Over the next three weeks, we'll be exploring issues that everyone can relate to – like press freedom, the plight of foreign domestic workers, racism, heritage, sex, love and politics.
You're directing two of the eight plays that will make their world premieres at the Festival. What has that experience been like?
Exhausting… but also exhilarating! Directing two plays at once is quite challenging! I've had to be very disciplined with my schedule, because I can go from a concept meeting for Faghag in the morning to a full run of Press Gang in the afternoon. Fortunately, I've been blessed with two fantastic creative and production teams who have helped me pull both shows together.
Working on brand-new plays is always exciting because you have a blank canvas. There's no precedent – no model from which you can take inspiration. The act of pure creation – bringing a play from page to stage – is scary, but also thrilling.
Let's turn to Press Gang. As the Festival's Co-Artistic Director, why did you commission this script?
We're living in interesting times. The press all over the world is under attack. Externally, from politicians like Donald Trump and the fact that you can get the news online. But internally too, especially in a country like Singapore. The press in our country isn't free. We all know that. But how much of that freedom is taken away – and how much is given away? How much self-censorship goes on in our newsrooms?
I commissioned Tarn How to write the play because he's one of our foremost playwrights – who was also a Straits Times journalist for 15 years! I knew he would have a really unique insight into this very Singaporean phenomenon. Also, we hardly have any plays about press freedom in Singapore – even though we rank 151st on the World Press Freedom Index! There's obviously plenty to say about that, right?
Ivan confers with playwright Tan Tarn How on a tricky moment in Press Gang
What are some of the challenges you faced in directing this production and bringing this script to life?
Tarn How's play is political. And by that, I don't just mean 'politics' as in 'politicians' – although that's present and accounted for. There's also small-p politics, like those in any organisation or bureaucracy. The characters are always on guard. There's an air of paranoia to the everyday. So each scene, each conversation, has its undertones of intrigue and power play. Playing politics all day is dirty but fun!
Will we recognise some of the characters in Press Gang?
Any resemblance to actual persons, living or dead, is purely coincidental… of course!
More seriously, what Tarn How has done is quite remarkable. The characters in his fictional newsroom truly represent a microcosm of Singaporean society. They cover our political spectrum: from the conservative to the liberal and radical; from the ignorant and apathetic and compromised, to those who are woke and trying to change the world.
What do you hope audiences take home with them after watching Press Gang?
I've always believed in the power of theatre to entertain as well as enlighten. So I hope our audiences have fun, first and foremost! But I also hope they will gain some insight into the relationship between the press and the government in Singapore. The media is supposed to keep us informed about what goes on in the world. If they don't, or can't, inform us about something we ought to know about, what implications does that have for us as individuals and as a society?
Ivan looks on as Pam Oei shares family photos and personal anecdotes for Faghag!
Last but certainly not least: what's it like working on Faghag with Pam Oei?
It's an absolute delight! Pam is one of my dearest friends, and also one of the most gifted performers I know. She's been talking about creating this one-woman show for years. So I gave her a deadline for this Singapore Theatre Festival, and here we are!
I'm really glad to have this opportunity to work with her on a script and a cause that's so close to both our hearts. In all the years I've known her, Pam has been a tireless champion of the LGBTQIA community. As a straight ally and a mother, she's always fought fiercely for equality and justice. As her director and as her friend, it's a privilege for me to give Pam this platform to tell her very personal story as 'Singapore's #1 Faghag'!
All Set To Go!
Becoming Emily of Emerald Hill
16 September 2019·
Dancing On Air

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text:
Kyle Busch's bid for more NASCAR history comes up short at Las Vegas
Ellen J. Horrow
For two days, Kyle Busch had a magical homecoming, and Sunday looked to be the icing on an already sweet cake.
The Las Vegas native had roared to victory in the Gander Outdoors Truck Series race Friday night then followed it up Saturday by rallying to win the Xfinity Series race in double overtime. There was only one box left to check at Las Vegas Motor Speedway — the Monster Energy NASCAR Cup Series race.
Only one driver has ever completed a weekend sweep of races in NASCAR's top three national series, and that driver did it twice. Of course, that driver is Busch, who pulled off the feat at Bristol Motor Speedway in 2010 and 2017.
But this one would be different. It would be in front of the hometown crowd where Busch is the hero and not the villain. It would be in front of family and friends, and it was there for the taking — until one minor gaffe derailed it all.
Busch was busted for entering pit road too fast during his green-flag pit stop in Stage 2 of the Pennzoil 400 and was forced to serve a pass-through penalty. He was leading the race before the pit stop and never got it back, despite a hard charge in the final stage that saw him rallying back to the front to finish third behind Team Penske's Joey Logano and Brad Keselowski.
"If we didn't have the speeding penalty on pit road, we would have won this race," Busch lamented after the race. "Overall we had a really fast car – the M&M's Camry was good and the driver threw it away."
Busch's demeanor during his post-race TV interview Sunday was in sharp contrast to the joyous driver who celebrated in victory lane the previous two days. And it seemed clear that the 2015 Cup Series champion understood that he had let an incredible opportunity slip from his grasp.
"I certainly screwed up our day coming to pit road there. We tried a different brake package for us this weekend — trying to make up time in order to get a bigger jump on the guys behind me coming to pit road there — and I just ruined it for us and we had to come from the back. I think we passed the most cars today, so I think we were the most impressive today, but that doesn't matter because we don't have a trophy. Whatever."
Busch remains three victories shy of 200 combined in Trucks, Xfinity and Cup. He'll go after win No. 198 next weekend at ISM Raceway in Avondale, Ariz.
This article originally appeared on USA TODAY: Kyle Busch's bid for more NASCAR history comes up short at Las Vegas


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Simply put, it's changing the way businesses handle their telecommunication needs because the infrastructure offered by Twilio is allowing web programmers to integrate real-time phone calls across a wide range of platform applications.
For developers it all comes down to a matter of exploiting open source programming which many companies are finding remarkable benefits from.
One of the most beneficial ways that Twilio is transforming the telecommunications industry is with its Pay-As-You-Go pricing structure. Under these terms a customer pays for the amount of cloud space capacity they need in the moment. In other words, there isn't any waste paying for extra storage or data compilation space when you don't need it.
Because Twilio's cloud solution eliminates programming, operational and contract hassles rapid growth is easier to come by. There won't be trouble with traffic spikes which is exactly what every company is hoping for. Twilio scales usage in both directions whether you experience highs or lows in your traffic.
Twilio cuts back on the learning curve needed to build out dependable voice communications applications. Think of this as "if it's not broke, don't fix it" approach to programming. Twilio is enabling developers to integrate business communication, VoIP and messaging right into web, desktop and mobile software applications.
There is no longer a need for a startup developer to square off against the telecom giants to help with the testing and developing phase of their products.
Twilio is bridging the gap for software developers to create new communication applications without the burdens of complexity and expense that might have proven to be a hindrance just a few years ago. This puts Twilio on the forefront of helping development quickly move on ideas that can be the most benefit to the end users. It is this kind of direct and rapid response to the development process in the cloud which is making Twilio the go to source for a wide range of mobile communication applications.


text:
package net.openhft.chronicle.core.util;

import net.openhft.chronicle.core.Jvm;
import net.openhft.chronicle.core.OS;
import net.openhft.chronicle.core.annotation.Java9;
import org.jetbrains.annotations.NotNull;
import org.jetbrains.annotations.Nullable;

import java.lang.reflect.Field;

import static java.lang.Character.toLowerCase;

public final class StringUtils {

    // Suppresses default constructor, ensuring non-instantiability.
    private StringUtils() {
    }

    private static final String VALUE_FIELD_NAME = "value";
    private static final String COUNT_FIELD_NAME = "count";
    private static final String CODER_FIELD_NAME = "coder";

    private static final Field S_VALUE;
    private static final Field SB_COUNT;
    private static final Field S_CODER;
    private static final Field SB_CODER;
    private static final long S_VALUE_OFFSET;
    private static final long SB_VALUE_OFFSET;
    private static final long SB_COUNT_OFFSET;
    private static final long S_COUNT_OFFSET;
    private static final long MAX_VALUE_DIVIDE_10 = Long.MAX_VALUE / 10;

    static {
        try {
            S_VALUE = String.class.getDeclaredField(VALUE_FIELD_NAME);
            Jvm.setAccessible(S_VALUE);
            S_VALUE_OFFSET = OS.memory().getFieldOffset(S_VALUE);
            if (Jvm.isJava9Plus()) {
                SB_CODER = Jvm.getField(StringBuilder.class.getSuperclass(), CODER_FIELD_NAME);
                S_CODER = Jvm.getField(String.class, CODER_FIELD_NAME);
            } else {
                S_CODER = null;
                SB_CODER = null;
            }
        } catch (Exception e) {
            throw new AssertionError(e);
        }

        long sCountOffset = -1;
        try {
            Field sCount = String.class.getDeclaredField(COUNT_FIELD_NAME);
            Jvm.setAccessible(sCount);
            sCountOffset = OS.memory().getFieldOffset(sCount);
        } catch (Exception ignored) {
            // Do nothing
        }
        S_COUNT_OFFSET = sCountOffset;

        try {
            final SbFields sbFields = new SbFields();
            SB_COUNT = sbFields.sbCount;
            SB_VALUE_OFFSET = sbFields.sbValOffset;
            SB_COUNT_OFFSET = sbFields.sbCountOffset;
        } catch (Exception e) {
            throw new AssertionError(e);
        }
    }

    private static final class SbFields {

        private Field sbValue;
        private long sbValOffset;
        private Field sbCount;
        private long sbCountOffset;

        public SbFields() throws ClassNotFoundException, NoSuchFieldException {
            try {
                sbValue = Class.forName("java.lang.AbstractStringBuilder").getDeclaredField(VALUE_FIELD_NAME);
                Jvm.setAccessible(sbValue);
                sbValOffset = OS.memory().getFieldOffset(sbValue);
                sbCount = Class.forName("java.lang.AbstractStringBuilder").getDeclaredField(COUNT_FIELD_NAME);
                Jvm.setAccessible(sbCount);
                sbCountOffset = OS.memory().getFieldOffset(sbCount);
            } catch (NoSuchFieldException e) {
                sbValue = Class.forName("java.lang.StringBuilder").getDeclaredField(VALUE_FIELD_NAME);
                Jvm.setAccessible(sbValue);
                sbValOffset = OS.memory().getFieldOffset(sbValue);
                sbCount = Class.forName("java.lang.StringBuilder").getDeclaredField(COUNT_FIELD_NAME);
                Jvm.setAccessible(sbCount);
                sbCountOffset = OS.memory().getFieldOffset(sbCount);
            }
        }
    }

    public static void setLength(@NotNull StringBuilder sb, int length) {
        try {
            SB_COUNT.set(sb, length);
        } catch (IllegalAccessException | IllegalArgumentException e) {
            throw new AssertionError(e);
        }
    }

    public static void set(@NotNull StringBuilder sb, CharSequence cs) {
        sb.setLength(0);
        sb.append(cs);
    }

    public static boolean endsWith(@NotNull final CharSequence source,
                                   @NotNull final String endsWith) {
        for (int i = 1; i <= endsWith.length(); i++) {
            if (toLowerCase(charAt(source, source.length() - i)) !=
                    toLowerCase(endsWith.charAt(endsWith.length() - i))) {
                return false;
            }
        }

        return true;
    }

    public static boolean startsWith(@NotNull final CharSequence source,
                                     @NotNull final String startsWith) {
        for (int i = 0; i < startsWith.length(); i++) {
            if (toLowerCase(charAt(source, i)) != toLowerCase(startsWith.charAt(i))) {
                return false;
            }
        }

        return true;
    }

    public static boolean isEqual(@Nullable CharSequence s, @Nullable CharSequence cs) {
        if (s instanceof StringBuilder) {
            return isEqual((StringBuilder) s, cs);
        }
        if (s == cs)
            return true;
        if (s == null) return false;
        if (cs == null) return false;
        int sLength = s.length();
        int csLength = cs.length();
        if (sLength != csLength) return false;
        for (int i = 0; i < csLength; i++)
            if (charAt(s, i) != charAt(cs, i))
                return false;
        return true;
    }

    private static char charAt(@NotNull CharSequence s, int i) {
        try {
            return s.charAt(i);
        } catch (IndexOutOfBoundsException e) {
            throw new AssertionError(e);
        }
    }

    public static boolean isEqual(@Nullable StringBuilder s, @Nullable CharSequence cs) {
        if (s == cs)
            return true;
        if (s == null) return false;
        if (cs == null) return false;
        int length = cs.length();
        if (s.length() != length) return false;

        if (Jvm.isJava9Plus()) {
            for (int i = 0; i < length; i++)
                // This is not as fast as it could be.
                if (s.charAt(i) != charAt(cs, i))
                    return false;
            return true;
        } else {
            char[] chars = StringUtils.extractChars(s);
            for (int i = 0; i < length; i++)
                if (chars[i] != charAt(cs, i))
                    return false;
            return true;
        }
    }

    public static boolean equalsCaseIgnore(@Nullable CharSequence s, @NotNull CharSequence cs) {
        if (s == null) return false;
        if (s.length() != cs.length()) return false;
        for (int i = 0; i < cs.length(); i++)
            if (Character.toLowerCase(charAt(s, i)) !=
                    Character.toLowerCase(charAt(cs, i)))
                return false;
        return true;
    }

    @Nullable
    public static String toString(@Nullable Object o) {
        return o == null ? null : o.toString();
    }

    public static char[] extractChars(StringBuilder sb) {
        if (Jvm.isJava9Plus()) {
            final char[] data = new char[sb.length()];
            sb.getChars(0, sb.length(), data, 0);
            return data;
        }

        return OS.memory().getObject(sb, SB_VALUE_OFFSET);
    }

    @Java9
    public static byte getStringCoder(@NotNull String str) {
        return getStringCoderForStringOrStringBuilder(str);
    }

    @Java9
    public static byte getStringCoder(@NotNull StringBuilder str) {
        return getStringCoderForStringOrStringBuilder(str);
    }

    @Java9
    private static byte getStringCoderForStringOrStringBuilder(@NotNull CharSequence charSequence) {
        try {
            if (charSequence instanceof String) return S_CODER.getByte(charSequence);
            else if (charSequence instanceof StringBuilder) return SB_CODER.getByte(charSequence);
            else return Jvm.getField(charSequence.getClass(), CODER_FIELD_NAME).getByte(charSequence);
        } catch (IllegalArgumentException | IllegalAccessException e) {
            throw new AssertionError(e);
        }
    }

    @Java9
    public static byte[] extractBytes(@NotNull StringBuilder sb) {
        ensureJava9Plus();

        return OS.memory().getObject(sb, SB_VALUE_OFFSET);
    }

    public static char[] extractChars(@NotNull String s) {
        if (Jvm.isJava9Plus()) {
            return s.toCharArray();
        }
        return OS.memory().getObject(s, S_VALUE_OFFSET);
    }

    @Java9
    public static byte[] extractBytes(@NotNull String s) {
        ensureJava9Plus();

        return OS.memory().getObject(s, S_VALUE_OFFSET);
    }

    public static void setCount(@NotNull StringBuilder sb, int count) {
        OS.memory().writeInt(sb, SB_COUNT_OFFSET, count);
    }

    @NotNull
    public static String newString(@NotNull char[] chars) {
        if (Jvm.isJava9Plus()) {
            return new String(chars);
        }
        //noinspection RedundantStringConstructorCall
        @NotNull String str = new String();
        try {
            S_VALUE.set(str, chars);
            if (S_COUNT_OFFSET > -1)
                OS.memory().writeInt(str, S_COUNT_OFFSET, chars.length);
            return str;
        } catch (Exception e) {
            throw new AssertionError(e);
        }
    }

    @Java9
    @NotNull
    public static String newStringFromBytes(@NotNull byte[] bytes) {
        ensureJava9Plus();
        //noinspection RedundantStringConstructorCall
        @NotNull String str = new String();
        try {
            S_VALUE.set(str, bytes);
            return str;
        } catch (Exception e) {
            throw new AssertionError(e);
        }
    }

    @Nullable
    public static String firstLowerCase(@Nullable String str) {
        if (str == null || str.isEmpty())
            return str;
        final char ch = str.charAt(0);
        final char c2 = Character.toLowerCase(ch);
        return ch == c2 ? str : c2 + str.substring(1);
    }

    public static double parseDouble(@NotNull CharSequence in) {
        long value = 0;
        int exp = 0;
        boolean negative = false;
        int decimalPlaces = Integer.MIN_VALUE;

        int ch = charAt(in, 0);
        int pos = 1;
        switch (ch) {
            case 'N':
                if (compareRest(in, 1, "aN"))
                    return Double.NaN;
                return Double.NaN;
            case 'I':
                //noinspection SpellCheckingInspection
                if (compareRest(in, 1, "nfinity"))
                    return Double.POSITIVE_INFINITY;

                return Double.NaN;
            case '-':
                if (compareRest(in, 1, "Infinity"))
                    return Double.NEGATIVE_INFINITY;
                negative = true;
                ch = charAt(in, pos++);
                break;
            default:
                // Continue below
        }
        while (true) {
            if (ch >= '0' && ch <= '9') {
                while (value >= MAX_VALUE_DIVIDE_10) {
                    value >>>= 1;
                    exp++;
                }
                value = value * 10 + (ch - '0');
                decimalPlaces++;

            } else if (ch == '.') {
                decimalPlaces = 0;

            } else {
                break;
            }
            if (pos == in.length())
                break;
            ch = charAt(in, pos++);
        }

        return asDouble(value, exp, negative, decimalPlaces);
    }

    private static void ensureJava9Plus() {
        if (!Jvm.isJava9Plus()) {
            throw new UnsupportedOperationException("This method is only supported on Java9+ runtimes");
        }
    }

    private static boolean compareRest(@NotNull CharSequence in,
                                       final int pos,
                                       @NotNull String s) {

        if (s.length() > in.length() - pos)
            return false;

        for (int i = 0; i < s.length(); i++) {
            if (charAt(in, i + pos) != s.charAt(i)) {
                return false;
            }
        }
        return true;
    }

    private static double asDouble(long value, int exp, boolean negative, int decimalPlaces) {
        if (decimalPlaces > 0 && value < Long.MAX_VALUE / 2) {
            if (value < Long.MAX_VALUE / (1L << 32)) {
                exp -= 32;
                value <<= 32;
            }
            if (value < Long.MAX_VALUE / (1L << 16)) {
                exp -= 16;
                value <<= 16;
            }
            if (value < Long.MAX_VALUE / (1L << 8)) {
                exp -= 8;
                value <<= 8;
            }
            if (value < Long.MAX_VALUE / (1L << 4)) {
                exp -= 4;
                value <<= 4;
            }
            if (value < Long.MAX_VALUE / (1L << 2)) {
                exp -= 2;
                value <<= 2;
            }
            if (value < Long.MAX_VALUE / (1L << 1)) {
                exp -= 1;
                value <<= 1;
            }
        }
        for (; decimalPlaces > 0; decimalPlaces--) {
            exp--;
            long mod = value % 5;
            value /= 5;
            int modDiv = 1;
            if (value < Long.MAX_VALUE / (1L << 4)) {
                exp -= 4;
                value <<= 4;
                modDiv <<= 4;
            }
            if (value < Long.MAX_VALUE / (1L << 2)) {
                exp -= 2;
                value <<= 2;
                modDiv <<= 2;
            }
            if (value < Long.MAX_VALUE / (1L << 1)) {
                exp -= 1;
                value <<= 1;
                modDiv <<= 1;
            }
            if (decimalPlaces > 1)
                value += modDiv * mod / 5;
            else
                value += (modDiv * mod + 4) / 5;
        }
        final double d = Math.scalb((double) value, exp);
        return negative ? -d : d;
    }

    @Nullable
    public static String toTitleCase(@Nullable String name) {
        if (name == null || name.isEmpty())
            return name;
        @NotNull StringBuilder sb = new StringBuilder();
        sb.append(Character.toUpperCase(name.charAt(0)));
        boolean wasUnder = false;
        for (int i = 1; i < name.length(); i++) {
            char ch0 = name.charAt(i);
            char ch1 = i + 1 < name.length() ? name.charAt(i + 1) : ' ';
            if (Character.isLowerCase(ch0)) {
                sb.append(Character.toUpperCase(ch0));
                if (Character.isUpperCase(ch1)) {
                    sb.append('_');
                    wasUnder = true;
                } else {
                    wasUnder = false;
                }
            } else if (Character.isUpperCase(ch0)) {
                if (!wasUnder && Character.isLowerCase(ch1)) {
                    sb.append('_');
                }
                sb.append(ch0);
                wasUnder = false;
            } else {
                sb.append(ch0);
                wasUnder = ch0 == '_';
            }
        }
        return sb.toString();
    }

    public static void reverse(StringBuilder text, int start) {
        int end = text.length() - 1;
        int mid = (start + end + 1) / 2;
        for (int i = 0; i < mid - start; i++) {
            char ch = text.charAt(start + i);
            text.setCharAt(start + i, text.charAt(end - i));
            text.setCharAt(end - i, ch);
        }
    }

    public static int parseInt(CharSequence s, int radix)
            throws NumberFormatException {
        /*
         * WARNING: This method may be invoked early during VM initialization
         * before IntegerCache is initialized. Care must be taken to not use
         * the valueOf method.
         */

        if (s == null) {
            throw new NumberFormatException("null");
        }

        if (radix < Character.MIN_RADIX) {
            throw forRadix(radix, true);
        }

        if (radix > Character.MAX_RADIX) {
            throw forRadix(radix, false);
        }

        int result = 0;
        boolean negative = false;
        int i = 0, len = s.length();
        int limit = -Integer.MAX_VALUE;
        int multmin;
        int digit;

        if (len > 0) {
            char firstChar = charAt(s, 0);
            if (firstChar < '0') { // Possible leading "+" or "-"
                if (firstChar == '-') {
                    negative = true;
                    limit = Integer.MIN_VALUE;
                } else if (firstChar != '+')
                    throw forInputString(s);

                if (len == 1) // Cannot have lone "+" or "-"
                    throw forInputString(s);
                i++;
            }
            multmin = limit / radix;
            while (i < len) {
                // Accumulating negatively avoids surprises near MAX_VALUE
                digit = Character.digit(charAt(s, i++), radix);
                if (digit < 0) {
                    throw forInputString(s);
                }
                if (result < multmin) {
                    throw forInputString(s);
                }
                result *= radix;
                if (result < limit + digit) {
                    throw forInputString(s);
                }
                result -= digit;
            }
        } else {
            throw forInputString(s);
        }
        return negative ? result : -result;
    }

    static NumberFormatException forInputString(CharSequence s) {
        return new NumberFormatException("For input string: \"" + s + "\"");
    }

    static NumberFormatException forRadix(int radix, boolean less) {
        if (less)
            return new NumberFormatException("radix " + radix +
                    " less than Character.MIN_RADIX");
        else
            return new NumberFormatException("radix " + radix +
                    " greater than Character.MAX_RADIX");
    }

    public static long parseLong(CharSequence s, int radix)
            throws NumberFormatException {
        if (s == null) {
            throw new NumberFormatException("null");
        }

        if (radix < Character.MIN_RADIX) {
            throw forRadix(radix, true);
        }
        if (radix > Character.MAX_RADIX) {
            throw forRadix(radix, false);
        }

        long result = 0;
        boolean negative = false;
        int i = 0, len = s.length();
        long limit = -Long.MAX_VALUE;
        long multmin;
        int digit;

        if (len > 0) {
            char firstChar = charAt(s, 0);
            if (firstChar < '0') { // Possible leading "+" or "-"
                if (firstChar == '-') {
                    negative = true;
                    limit = Long.MIN_VALUE;
                } else if (firstChar != '+')
                    throw forInputString(s);

                if (len == 1) // Cannot have lone "+" or "-"
                    throw forInputString(s);
                i++;
            }
            multmin = limit / radix;
            while (i < len) {
                // Accumulating negatively avoids surprises near MAX_VALUE
                digit = Character.digit(charAt(s, i++), radix);
                if (digit < 0) {
                    throw forInputString(s);
                }
                if (result < multmin) {
                    throw forInputString(s);
                }
                result *= radix;
                if (result < limit + digit) {
                    throw forInputString(s);
                }
                result -= digit;
            }
        } else {
            throw forInputString(s);
        }
        return negative ? result : -result;
    }
}

redpajama_set_name: RedPajamaGithub


Welcome to Little Wildflowers! My name is Anya Grace. My husband and I use our business as a way to express our passion for the arts, health, and educating and supporting families in their walks with God.
We are passionate worshipers and ministers in everything we do in life, whether it be through music, our careers or through parenting. God is our greatest love! And the children He has blessed us with are the most amazing little men I have ever met. Let us serve you! Become a part of our journey through this crazy, messy, amazing life and grow closer to God WITH us!
May God have the glory and may you fall head over heals in love EVERY day with our incredible Lord Jesus Christ! What an abundant life He has given us!


text:
Q: Is there any way to check if text is inside html tag? Let suppose I need to extract every text from specific html tag:
HTML:

var subject = document.getElementById('subject').innerHTML;
console.log(subject); //

So we don't have any text inside, but if there is - how to check if there is text outside of <> tags inside our specific html element?
fiddle for better visualization - http://jsfiddle.net/kxarc6o3/

A: The best way is to go for innerText, innertHTML gives you the entire content within the tag including the html tags it holds and the html its child or decendents holds.
innerText always gives you the text it contains(only the element not its decendents).
in your example
hellohi

document.getElementbyID('spanid').innerText will only give hello, as a string
whereas document.getElementbyID('spanid').innerHTML will give the entire hmtl contains it has inside it (here hellohi ) in a string format.
To get innerText of all possible elements inside the span tag you need to use recursion, there is no other way as we dont know how many children or decedents it has.
printInnerText(ele){
 if(ele.childNodes.length >= 1){
    children = ele.childNodes;
    for(var i=0;i<children.length;i++)
     printInnerText(children[i])
 }else{
    console.log(ele.innerText);
 }
}

A: You can use HTML DOM innerHTML property like this:
if(document.getElementById("container").innerHTML.length > 0)
    console.log(document.getElementById("container").innerHTML);

Or using Jquery:
if($("#container").html().length > 0)
    console.log($("#container").html());

redpajama_set_name: RedPajamaStackExchange


text:
$350bn investment, tech to transform Mena leisure industry
Technology will be the key driver
$350bn tech investment to transform Mena leisure industry
DUBAI: The region's leisure tourism sector is showing signs of recovery, says the Middle East North Africa Leisure Attractions Council (Menalac) as it organises the LEA Conference and Annual Awards Ceremony on Tuesday November 10, 2020.
The Middle East's Leisure Entertainment and Amusement Industry that is undergoing digital transformation will be the fastest in the world to recover from the Covid-19 pandemic early next year, according to Menalac.
With the support of all its sponsors, Menalac had made the decision to go ahead with these events as the Middle East is seeing plans for massive developments across the leisure entertainment and attractions industry with forecast investment of more than $350 billion in the theme parks and attractions, according to reports.
With a clear indication that the socio-economic fundamentals of the Middle East where a high proportion of the population are young remains extraordinarily strong, it is expected that this highly tech-savvy young generation will be the drivers of adopting technology across the industry moving forward.
Digital and contactless technology is expected to play a dominating role in transforming the $80.58 billion (AED295.72 billion) leisure attractions industry in the Middle East and North Africa (Mena) region as the sector recovers from Covid-19. The region's theme parks are currently getting busier with a growing number of visitors, following the gradual re-opening of most of the parks and especially with the change in the weather.
The Middle East and North Africa Leisure Attractions Council (Menalac) expects the industry to transform itself to become future-ready with technology adoption, as personalisation, safety, security, and wearable gadgets dominate the future trends in the industry.
Mishal Al Hokair, Deputy CEO of Al Hokair Group, says: "Entertainment is always trendy and developing all the time. Therefore, I do recommend studying the market well before you choose which type of entertainment you will go with. All the fields in entertainment are attractive especially sport, e-sport, and family entertainment centres.
"Training and development in all aspects is crucial and the owner should always educate him/herself. Don't forget to plan for a good budget on IT and online products."
Middle East theme park and attraction operators are heavily investing in technology to create fully immersive and connected guest experiences they cannot get anywhere else. The various experience upgrades that the industry in the Middle East are investing in include the deployment in digital ticketing, cloud-base solutions, digital payment, augmented and virtual reality and experiential attractions.
The Middle East's Leisure and Attractions industry will increasingly deploy Artificial Intelligence, Virtual Reality (VR) technologies – including VR-based rides.
Sheikha Monira Al Sabah, CEO of Play Enterprises and Co-Founder of Trampo Extreme, says: "The modern-day family entertainment industry incorporates with it a sizeable factor of technology now more than ever. Whether it is arcade games, virtual reality games and rides, augmented reality games, touch screen or even laser tag style games among others.
"With technology developing at a more rapid pace today, we have to keep up with these developments to ensure our customers have these modern-day experiences. People do not have to be well travelled anymore to know what the latest trends are in the US, UK or Asia as they can see them from a click of a mobile phone and browse for this information online. Therefore, we must always assume that our customers will know what is the latest the industry has to offer and provide it to them in a timely fashion. You do not want to be viewed as outdated."
International visitor impact in the Middle East was estimated at $102 billion (Dh375 billion) in 2019, of which 79% is in the leisure industry, according to the World Travel and Tourism Council (WTTC).
Jean Habre, CEO of Abdullah Al Othaim Leisure and Tourism Co, says: "Lots of digitisation and technology will come into operations, such as iTeller, digitised entry and forms, RFID wristbands, E-tickets for redemption, etc. We are going to see more contactless procedures in place including e-commerce, self-service payment and redemption kiosks will have more impetus.
"Since customers are more safety and hygiene centric, the operators have to ensure follow the revised Standard Operating Procedures (SOPs). Customers will look for more value as spending power has changed; so operators will have to be innovative in providing extra value through hospitality or food and beverage partners."
Global accounting firm PricewaterhouseCooper (PwC) forecasts that the leisure and entertainment industry in the UAE has a market potential that will reach 45 million visitors by 2021. Of the Middle East's diverse verticals in tourism, one that stands out for its immense potential is that of theme parks. As per pre-Covid-19 estimates, the Dubai theme parks industry could generate about $5 billion (Dh18.3 billion) as annual revenue by 2020.
Dave Sandstorm, Vice President, International Sales at Bob's Space Racers, says: "Touch free entertainment, more cashless payment options, social distance entertainment and cleaning solutions will dominate the trends within the industry. We had a great prosperous industry before the pandemic hit us. Be patient it will be back stronger than ever!"
Renee Welsh, CEO of Embed for the EMEA region, says: "Endless research studies confirm that a new type of customer is emerging from the pandemic. They are more conscious of hygiene and safety than ever before, so they are only going to businesses with clear safety policies, like check-in (for tracking and tracing purposes), temperature checks at the door, mandatory mask-wearing, implementation of safety measures (like protective gear for staff), social distancing measures, hand sanitisation stations in the venue, capacity management, and contactless payment solutions.
"In fact, the pandemic has forced the world to enter the 'Low-touch Economy'. Every individual on the planet is more conscious about hygiene than ever before. Around 82 percent of people view contactless and low-touch as the safest way to pay, which is why you've seen a dramatic spike in Mobile Payments using the Mobile Wallet.
"Consumers have peace of mind and feel more secure keeping their mobile phones clean and hands sanitised than trusting a surface area that has been cleaned by a business with high foot traffic. Mobile usage, including payments, is an immutable force around the globe. Low-touch and contact-free payments and game-play are a safety measure that enables businesses to mitigate health risks related to Covid-19."
Rosa Tahmaseb, Secretary General of Menalac, added: "In addition to these trends, new international amusement parks and brands are expected to open in the region within the next few years and this will clearly help in the recovery of both regional and international tourism. Moving forward we envisage that whilst long haul holidays will remain on the to do list for some families, many will be spending their free time seeking holiday destinations closer to home. For the Mena region with a high population of young teens and young adults their expectations for high quality attractions and entertainment with a strong emphasis on technology will help shape the future of how technology will be a key player in the transformation of the Leisure & Attractions industry across the Mena region."
The sponsors for this year's events are all highly respected operators and suppliers to the industry, their support for these events is indicative of the positive feelings being shared in regard to the expected recovery of the Leisure & Attractions industry across the Mena region.
Al Hokair Group, one of the founding members of Menalac is also its Diamond Sponsor for the Menalac Awards 2020. Al Hokair Entertainment is one of the largest operators in Saudi Arabia's family entertainment industry with 64 entertainment centres around the kingdom in addition to operations across the Middle East.
As Gold sponsors, Menalac Awards has some big players involved, these include Cheer Amusement, a highly renowned indoor playground equipment manufacturer and Abdullah Al Othaim Leisure and Tourism Co. a popular name, creating benchmark Family Entertainment Destinations across many cities in Saudi Arabia and the Middle East.
Play Enterprises a highly respected Family Entertainment Centre operator based in Kuwait supports both the events as the Tittle Sponsor of the Menalac Conference and Silver Sponsor for the Awards Ceremony. There is also Bob Space Racers as a Silver sponsor for the Awards Ceremony, with over four decades of experience providing games and management services for the arcade, park, and trailer industries throughout the world.
Embed, the Technology partner of Menalac Conference and Awards, is a worldwide leader of cashless business management solutions with Mobile Wallet, Kiosks, Card Readers, Game Cards, POS Systems.
Rosa Tahmaseb, Secretary General of Menalac, says: "Menalac will bring together top industry experts and stakeholders at the Virtual Leisure Entertainment and Amusement (LEA) Conference and Awards Ceremony to talk about the key issues, challenges and trends in the industry as well as hold panel discussions aimed at highlighting the industry's achievement and future growth."
Thanking the government and sponsors for their support, she continues: "I would like to thank the government authorities who have supported the reopening of the industry across the Mena region while ensuring a strong focus remains on providing safe environments for guest to visit. I would also like to thank our esteemed sponsors for supporting the Virtual LEA Conference and Awards Ceremony at such a crucial time."
Menalac is the key representative organisation for the entire leisure entertainment and amusement industry in the Middle East and North Africa (Mena) region. With over 470 operations and 200 brands from over 22 countries in the Mena region in addition to Pakistan and Afghanistan, Menalac offers great benefits to the industry as a platform for stakeholders to interact and stay informed. -- Tradearabia News Service


Where are the best places to do these at?
Does anyone have any whale watching suggestions pls?
Where's the best but also least expensive all-inclusive resort?
Images from the Best Carnevals in the D.R.
Best Ob/gyn and clinic in Sosua/Puerto Plata area?
Best luxury car rental near POP airport?
Where to buy the best coffee from the DR?
Anything going on from 10/22-10/31/14?
Carnivale season here in d.r.
best part of dr for vacationing (on a budget)?
Taxi to Entrance of Samana Hwy or Bus Station in SDQ?
Who will be having the best Super Bowl Party?
Best cake shop near Zona Colonial?


Kombucha's exact origins aren't really known, but what we do know is that this either slightly sweet or sour refresher is super good for you, and a real taste bud zinger too. Created by a natural fermentation process, and containing a living culture that ferments and eats up the tea and sugar (SCOBY), it's brewed with Chun Mee Green Tea with a medley of sweet and tangy wild berries thrown in. Soft drinks, be gone.
Filtered water, Raw Cane sugar*, Chun-Mee green tea*, Hibiscus*, Licorice Root*, Rosehip*, Nettle*, Pineapple*, Natural Flavourings, Bilberry*, Kombucha culture* * = produced to organic standards.


My twenty-sixth stadium of 2011 was on Thursday 14th April 2011 at Boundary Stadium in South Oxhey, Hertfordshire. The match was Oxhey Jets vs. Leverstock Green in the West Hertfordshire St. Mary's Cup Semi-Final.
Boundary Stadium is just under a mile from Carpenders Park station on the London Overground network. The ground is sat next door to a community swimming pool and is surrounded by a residential area on one side and fields on the other. The stadium has three stands - two running alongside the pitch on the west side of the ground and one behind the goal in the north side of the ground.
The stand on the north side is just a general standing area covered by a roof while the two stands on the west side provide seating. One is a small structure with benching while the main stand (the Elliott Family Memorial Stand) which can hold around 100 people is split in two by the players entrance which leads from the changing rooms to the pitch. Next to this there is a raised concrete terrace section for fans to get the best view from.
The tie was the semi-final of the West Hertfordshire St. Mary's Cup - a small local competition consisting of just eight teams. The two teams that were involved in this semi-final both play their football in the Spartan South Midlands League Premier Division, with Leverstock Green towards the top end of the table and Oxhey Jets struggling near the bottom.
The game started with a quick goal for Leverstock which was scored from the edge of the box after just 3 minutes. Oxhey were able to equalise after a goalkeeping error half an hour in, but Leverstock managed to scramble the ball into the net just before half-time to make it 2-1 to the visitors at the break. The second half was evenly poised until the 75th minute when Leverstock scored a well taken third. This seemed to break Oxhey's spirit and they soon conceded a fourth. Leverstock added a fifth in stoppage time to complete a comprehensive victory over the home side.


Posted by Ted Guarnero admin on Sunday, December 20th, 2009 at 10:49am.
Chicago is a very dog friendly city with many pet friendly buildings. However, would you believe that one of the friendliest is also one of Chicago's most luxurious buildings?
Trump International Hotel & Tower has quickly become known as Chicago's premier luxury building and has attracted some of the country's most exclusive residents and their four legged friends. Trump Tower currently has no weight restriction on dogs and allows multiple dogs per unit. The building also features a new dog park right on site allowing you to not have to go very far to walk your best friend, even on the darkest of nights.
While it is unclear the exact number of dogs currently living in luxury at Trump Tower, the number is definitely great. A short ten-minute sit in the residential lobby will more than likely guarantee you several dog sightings as residents and dog walkers hit the streets or the dog park.
The building is known for having luxurious master suites. All three bedroom units feature fireplaces in the master bedroom, while some master suites have not only his and hers closets, but his and her bathrooms as well.
As a resident of Trump Tower, whether you own or rent, you are entitled to full access to all hotel amenities. The health club features morning yoga classes and the in-room dining even has a special menu just for your dog.