Your Huawei P20 Pro may need extra settings if you want to use voice mail with your BASE SIM card. In some cases, voice mail is automatically configured upon first use of the SIM card.
Under SIM 1, choose Additional settings.


Words and Noise: Fables Out Of Nyanja Out!
Fables Out Of Nyanja Out!
The release of a book is not something that happens out of the blue, without the writer knowing. Much as it is the publisher who determines many of the details of the release of the book, the writer most of the time knows when the book will be released. The process of writing and being published, the process of conception and giving birth to a book under normal circumstances should prepare the writer for that moment when their book is released.
That is what I thought before 1st, March 2012. Fables Out Of Nyanja was released this week and I am a bit embarrassed that I, of all people can't find the words to describe the feeling of having the book out, available for those who want, to have a read. I can however tell those who want a read where they can find the book. Amazon and other online bookstores, while they have not yet updated their listings, have the book.
In the meantime, you can have some love from Kushinda, the book's publishers who are selling it on their online Book store. They are in fact offering you free postage on buying the book through their online book store. Just click here and you will be sorted.
oh my goodnesss.... I am so so so so proud of you. So proud. I cant wait to get a hold of the copy and read it.. I just can not.
God Bless and I am excited and again proud of you!


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

Over the last six years, the LIGO \citep{aasi2015} and Virgo \citep{acernese2015}
interferometers dectected an increasing number of gravitational wave (GW) events \citep[e.g.,][]{abbottO1,abbottGW150914,abbottO2,abbottGWTC2.1}. At the end of the third observing run,
the third GW transient catalog (GWTC-3) consists of 90 GW candidates \citep{O3b,O3population}.
Most of these events are produced by the inspiral of two
black holes (BHs). Among the most peculiar  events, the merger remnant of GW190521 \citep{abbottGW190521,abbottGW190521astro} is the first  intermediate-mass black hole (IMBH) ever detected in the mass range $100-1000 \, \mathrm{M_{\odot}}$, with a remnant mass of $142^{+28}_{-16} \, \mathrm{M_{\odot}}$.
Also, GW190412 \citep[][]{abbottGW190412} represents the first observation of a BBH with asymmetric masses. The population of mergers in GWTC-3 also includes two binary neutron star (BNS) mergers, $\mathrm{GW170817}$ and  $\mathrm{GW190425}$ \citep{abbott170817mm,abbott170817grb,abbottGW190425}, and two black hole-neutron star (BHNS) candidates,  $\mathrm{GW200105\_162426}$ and $\mathrm{GW200115\_042309}$ \citep{abbottBHNS}. Furthermore, \cite{nitz2021} and \cite{olsen2022} reported several additional GW candidates \citep[see also][]{venumadhav2019,venumadhav2020,nitz2020,nitz2021}.

The abundance of detected GW sources allows us to attempt to reconstruct their formation channels. In fact,
thanks to the distinctive features that different formation channels imprint on the merging progenitors, even a few hundreds detections may be sufficient to identify their main formation pathways \citep{fishbach2017, zevin2017,stevenson2017,farr2017,vitale2017,gerosa2017,gerosa2018,bouffanais2019,bouffanais2021a,bouffanais2021b,wong2019,wong2020,zevin2020,doctor2020,kimball2020,ng2020}.
The isolated formation scenario, for example, predicts the formation of BBHs with primary masses up to $40-50 \, \mathrm{M_{\odot}}$, mostly equal-mass systems, with preferentially aligned spins and vanishingly small eccentricity in the LIGO--Virgo band \citep{mandel2016,gerosa2018}. According to this scenario, the formation of tight enough binary black holes (BBHs) can take place through evolutionary processes like common envelope \citep{tutukov1973, bethe1998,portegieszwart1998,belczynski2002, belczynski2008,belczynski2010,dominik2012, dominik2013,
mennekens2014, loeb16,belczynski2016,demink2016,marchant2016,
mapelli2018,mapelli2019, giacobbo2018b,
kruckow2018,spera2018,tang2019,belczynski2020,garcia2021}, chemically homogeneous evolution \citep{demink2016,mandel2016,marchant2016,dubuisson2020}, or stable mass transfer \citep[e.g.,][]{giacobbo2018,neijssel2019,bavera2020}.

The dynamical formation scenario, instead, involves dynamical processes in dense stellar environments,
like young star clusters \citep[YSCs, e.g.,][]{portegieszwart2002,sambaran10,mapelli2013,ziosi2014,goswami2014, mapelli2016, banerjee2017, banerjee2018,rastello2018,perna2019,
dicarlo2019,dicarlo2020,kumamoto2019,kumamoto2020,banerjee2020,rastello2020,rastello2021,dallamico2021,chattopadhyay2022},
globular clusters \citep[e.g.,][]{downing2010,BenacquistaDowning2013,rodriguez2015,rodriguez2016,antonini2016,
askar2017, fujii2017,askar2018,fragione2018,rodriguez2019} and nuclear star clusters \citep[e.g.,][]{oleary2009,millerlauburg2009,mckernan2012,megan17,mckernan2018,vanlandingham2016,
stone2017,hoang2018,arcagualandris2018,antonini2018,arcasedda2019,arcasedda2020,mapelli2021}.
With respect to the isolated channel, this scenario predicts the formation of merging BBHs with larger primary masses
\citep[e.g.,][]{mckernan2012,mapelli2016,antonini2016,gerosa2017,stone2017,mckernan2018,dicarlo2019,dicarlo2020,rodriguez2019,yang2019,arcasedda2019,arcasedda2020,mapelli2021b},
isotropic spin distributions \citep[e.g.,][]{rodriguez2016b}, and, in some rare cases, non-zero eccentricity in the LIGO--Virgo band \citep[e.g.,][]{samsing2018,samsing2018b,samsing2018c,rodriguez2018,zevin2019,dallamico2021}.

In this work, we will focus on the dynamical formation of BBHs  in young
and open stellar clusters. These systems are of key importance to interpret the formation of
BBHs, because they host the formation
of the most massive stars \citep{lada2003,portegieszwart2010,crowther2010}, which are the progenitors of massive BHs. Thanks to the high central densities of the host cluster ($\rho \gtrsim 10^{3} \, \mathrm{M_{\odot} pc^{-3} }$, \citealp{portegieszwart2010}), binary stars can efficiently interact with the surrounding stars since the very beginning of their life. This leaves a deep imprint on the properties of the population of BBHs and, in turn, merging BBHs. When YSCs are eventually disrupted by the tidal field of their host galaxy, their stellar content is released into the galactic field. Thus, a large fraction of BBHs which are now in the field may have formed in young stellar systems.

The dynamical formation and evolution of BBHs in YSCs are explored in a realistic way by means of direct $N-$body simulations, where up-to-date prescriptions for single and binary stellar evolution are implemented. In many cases, only the first few hundreds Myr of the life of the star cluster are considered. This is due, on the one hand, to their small relaxation timescales,
$t_{\mathrm{rlx}} \lesssim 100 \, \mathrm{Myr}$ \citep{portegieszwart2010}. In particular, the rapid decrease of their central density within the first Myr suppresses the interaction rate in later phases, making them less and less important in shaping the BBH properties.
On the other hand, producing large sets of $N-$body simulations, which are necessary to explore the population of merging BBHs with sufficient statistics, has high computational costs. Thus, evolving large sets of YSCs for thousands of Myr would turn to be prohibitively expensive. As a consequence, many simulation of YSCs only take into account the first 100 Myr of the star cluster life \citep{,dicarlo2019,dicarlo2020,dicarlo2020b,rastello2020,rastello2021}.

The aim of this work is to evaluate the impact of the late phases (up to $1500 \, \mathrm{Myr}$) of the dynamical evolution of the star cluster on the population of BBH mergers. To this purpose, we have run two sets of $N-$body simulations of YSCs in different mass regimes and studied the evolution of the population of BBHs.
To calculate the impact of the long-term evolution of the cluster, we compared the BBH merger populations at two different snapshots, $100 \, \mathrm{Myr}$ and $1500 \, \mathrm{Myr}$. The paper is organized as follows: in Section~\ref{sec_methods}, we describe the details of the $N-$body simulations and our method. In Section~\ref{sec_results}, we report the results for the BBH populations and mergers. Finally, Section~\ref{sec_conclusions} summarises our conclusions.

\begin{figure*}
\begin{center}
\includegraphics[width=\textwidth]{plots/radii_median_new.pdf}
\caption{
Evolution of the half-mass radius $r_{\mathrm{h}}$ (upper panels, solid lines), core radius $r_{\mathrm{c}}$ (lower panels, solid lines), and tidal radius $r_{\mathrm{t}}$ (dashed lines) for low-mass clusters (left) and high-mass clusters (right). Each set is divided into three subsets: for the low-mass clusters $M_{\mathrm{SC}} \in$ [500, 600] M$_\odot$ (violet), [600, 700] M$_\odot$ (green), [700, 800] M$_\odot$ (yellow). For the high-mass clusters $M_{\mathrm{SC}} \in$ [5000, 6000] M$_\odot$ (violet), [6000, 7000] M$_\odot$ (green), [7000, 8000] M$_\odot$ (yellow). Each line shows the median value over the simulated YSCs per each mass bin. The black lines (right panels) refer to the same physical quantities for the star clusters with $M_{\mathrm{SC}} =5\times10^4 \, \mathrm{M_{\odot}}$.
}\label{fig_radii}
\end{center}
\end{figure*}

\begin{figure}
\begin{center}
\includegraphics[width=\hsize]{plots/Mfin_Min_histograms.pdf}
\caption{Distribution of the ratio between the star cluster bound mass at the end of the simulation, $M_{\mathrm{SC,f}}$, and its initial mass $M_{\mathrm{SC}}$, for stellar systems with initial mass $M_{\mathrm{SC}} \in$ [500, 800] M$_\odot$ (violet), [5000, 6000] M$_\odot$ (blue), [6000, 7000] M$_\odot$ (green), [7000, 8000] M$_\odot$ (yellow), and  $M_{\mathrm{SC}} = 5 \times 10^4 \, \mathrm{M_{\odot}}$ (black).}\label{fig_mfin}
\end{center}
\end{figure}

\section{Methods}\label{sec_methods}

\subsection{Direct \textit{N}-body code} \label{sec_nbody}

We performed our simulations
with the $N-$body code \textsc{nbody6++gpu} \citep{wang2015,wang2016}, coupled with the population synthesis code\footnote{{\sc mobse} is publicly available at \href{http://demoblack.com/catalog_codes/mobse-public-version/}{this link}.} \textsc{MOBSE} \citep{mapelli2017,giacobbo2018,giacobbo2018b}.
\textsc{nbody6++gpu} is the \text{GPU} parallel version of \textsc{nbody6} \citep{aarseth2003}.
It implements a 4th-order Hermite integrator, individual block time-steps \citep{makino1992} and Kustaanheimo-Stiefel regularization of close encounters and few-body systems. The force contributions at short time steps (\textit{irregular forces}) are computed by a  neighbour scheme \citep{nitadori2012}, and for long time steps (\textit{regular} force/timesteps) the force is evaluated by considering all the particles of the system. The irregular-force calculation is performed using CPUs, while the regular forces are evaluated on GPUs using the CUDA architecture.
A solar neighbourhood-like static external field \citep{wang2016} is included in the force integration. This choice for the tidal field is quite conservative, because the static tidal field does not take into account possible perturbations by disk- and bulge-shocking and encounters with molecular clouds, which can accelerate the star cluster disruption \citep{gieles2006}.
Orbital decay and circularization by GW emission are calculated following \cite{peters1964}.
Post-Newtonian terms are not explicitly included in this version of the code.

\textsc{mobse} is a customized and upgraded version of \textsc{bse} and includes up-to-date prescription for massive stellar winds \citep{giacobbo2018}, core-collapse \citep{fryer2012} and electron-capture supernovae \citep{giacobbo2018c}, natal kicks \citep{giacobbo2020} and (pulsational) pair instability supernovae \citep{mapelli2020b}.
Stellar winds are modeled by assuming that the mass loss of hot massive stars depends on metallicity as $\Dot{M} \propto Z^{\beta}$, where $\beta$ is modelled as in \cite{giacobbo2018}.

For this work, we adopt the delayed model for core-collapse supernovae from \cite{fryer2012}. In this model, there is no mass gap between neutron stars and BHs: we assume that compact objects more massive than 3 M$_\odot$ are BHs. Natal kicks are modeled according to the prescription by  \cite{giacobbo2020}: the magnitude of the kick can be expressed as $v_{\mathrm{kick}} \propto f_{\mathrm{H05}} \, m_{\mathrm{ej}} \, m_{\mathrm{rem}}^{-1}$, where $f_{\mathrm{H05}}$ is a random number drawn from a Maxwellian distribution with a one-dimensional root mean square velocity $\sigma = 265 \, \mathrm{km \, s^{-1}}$,  $m_{\mathrm{rem}}$ is the mass of the remnant, and $m_{\mathrm{ej}}$ is the difference between the final mass of the star before the supernova explosion and the mass of the remnant. Binary evolution processes (tides, mass transfer, common envelope and GW-orbital decay) are implemented as in \cite{hurley2002}. The common envelope process is implemented by adopting the energy formalism \citep{webbink1984}. In this case, we assume $\alpha=3$, while the concentration parameter $\lambda$ is calculated self-consistently as in \cite{claeys2014}.

\subsection{Initial conditions for star clusters} \label{sec_initial_coditions}

\begin{figure*}
\begin{center}
\includegraphics[width=\textwidth]{plots/bbh_ALL_histograms.pdf}
\caption{Mass distribution of BHs in BBHs, for low-mass clusters (left) and high-mass clusters (right).
Red line: original BBHs at 1500 Myr.  Orange filled histogram: original BBHs at 100 Myr. Blue dashed line: exchanged BBHs at 1500 Myr.  Light blue hatched histogram: exchanged BBHs at 100~Myr.
Among the original BHs, we highlight in red those with mass in the PI mass gap at 1500 Myr (red dash-dotted line) and at 100 Myr (red filled histogram).}\label{fig_all_bbh}
\end{center}
\end{figure*}

\subsubsection{Stellar and binary populations}

We generate the initial masses of stars (single stars, primary and secondary members of binary systems)  according to a \cite{kroupa2001} initial mass function between $0.1 \, \mathrm{M_{\odot}}$ and $150 \, \mathrm{M_{\odot}}$. We assume a metallicity $Z=0.002$, approximately corresponding to $0.1$ Z$_\odot$.
For binary systems, we assume a distribution of mass ratios  $\mathcal{F}(q) \propto q^{-0.1}, \;  \mathrm{with} \; q \; \in [0.1,\,{}1]$ \citep{sana2012}. Also, our algorithm generates a binary fraction that matches the observational results by \cite{moe2017}. In  this work, the binary fraction for the primary mass in the different mass bins (expressed in solar masses)
is set to: $f_{b,[0.1,0.8]}=0.20$, $f_{b,[0.8,2]}=0.40$,  $f_{b,[2,5]}=0.59$, $f_{b,[5,9]}=0.76$,  $f_{b,[9,16]}=0.84$, $f_{b, [16,150]}=0.94$.
We generate the orbital parameters of binary systems following the observational prescriptions by \cite{sana2012}.
In particular,  we randomly draw the orbital periods from: $\mathcal{F}(\mathcal{P}) \propto \mathcal{P}^{-0.55}, \; \mathrm{with} \; \mathcal{P}=\log_{10}(P/ {\rm days})\in [0.15,\,{}5.5], $
and the eccentricities from $\mathcal{F}(e) \propto e^{-0.45}, \; \mathrm{with} \; e \in [10^{-5},\,{}e_{\rm max} (P)]
$.
For a given orbital period, we set an upper limit for the eccentricity distribution according to \cite{moe2017}: $e_{\rm max} (P) = 1 - \left[ P / (2 \, {\rm days}) \right]^{-2/3}$. We refer to \cite{torniamenti21} for more details on our binary population.

\subsubsection{Stellar clusters}

We initialize stellar positions and velocities in the simulated  YSCs
with fractal initial conditions, with a fractal dimension $D=1.6$, in order to mimic the observed clumpiness of embedded star clusters \citep{cartwright2004,sanchez2009, kuhn2019}.  We generate fractal phase space distributions with {\sc Mcluster} \citep{kuepper2011}.

We uniformly sample the half-mass of our star clusters  between 0.5 and 2 pc  \citep[e.g.,][]{portegieszwart2010,krumholz2019}.
To evaluate the impact of long-term dynamics on the properties of BBH mergers in different dynamical regimes, we consider two sets of star clusters in different mass ranges ($M_{\mathrm{SC}}$):
\begin{itemize}
    \item {\emph{Low-mass star clusters}}, with mass ranging from $500 \, \mathrm{M_{\odot}}$ to  $800 \, \mathrm{M_{\odot}}$. These clusters present short dynamical evolution timescales at all scales: this reduces the probability of dynamical interactions and, consequently, of dynamical exchanges. Also, YSCs in this mass range typically host a few massive stars, and, consequently, BHs. This further suppresses the rate of dynamical exchanges\footnote{Because the observed binary fraction increases with the mass of the primary star, the most massive stars are typically born in binary systems. If few or no single BHs are present, dynamical exchanges are limited because the probability of an exchange is strongly suppressed if the intruders are less massive than the two members of the binary system.} \citep{rastello2021}.

    \item {\emph{High-mass star clusters}}, with mass ranging from $5000 \, \mathrm{M_{\odot}}$ to $8000 \, \mathrm{M_{\odot}}$. These clusters have a higher rate of dynamical encounters, as a consequence of the higher densities,

    longer dynamical timescales and
    larger number of massive stars. Thus, they are expected to produce a larger number of exchanged binaries and BBHs (\citealp{rastello2021}).  In this sample we also include two star clusters with mass $5\times 10^4 \, \mathrm{M_{\odot}}$.

\end{itemize}
In both cases, we sample the mass of star clusters from a power-law distribution $dN/dM_{\mathrm{SC}} \propto M_{\mathrm{SC}}^{-2}$, following \cite{lada2003}. The two sets consist in 35578 and 3555 star clusters, respectively. The number of star clusters in the two samples is set to obtain the same total mass. The total kinetic ($K$) and potential ($W$) energy of the cluster are set to give a virial ratio $q=2\,{}K/W=1$.

\begin{figure*}
\begin{center}
\includegraphics[width=\textwidth]{plots/binary_formation_histograms_combined.pdf}
\caption{Distribution of formation times ($t_{\mathrm{form}}$) of binary systems that give birth to exchanged BBHs, in low-mass clusters (left) and high-mass clusters (right). Upper panels: all exchanged BBHs. Lower panels: exchanged BBH mergers. Blue dashed line and hatched area: BBHs that formed when both components were stars. Orange dot-dashed line: BBHs that formed when one component was a star and the other was a BH. Black line: BBHs that formed when both components were BHs. Grey area: all BBHs.}\label{fig_bin_form}
\end{center}
\end{figure*}

\subsection{Impact of long-term evolution}

The main goal of this work is to evaluate the impact of the long-term dynamical evolution,
up to $1500 \, \mathrm{Myr}$. In particular, we compare the population of BBH mergers that form in the first 100 Myr of the evolution of the simulated YSCs with the population of BBH mergers at 1500 Myr.

We first evaluate the population of BBH mergers that we would have obtained if we had integrated the evolution of our YSCs only for the first 100 Myr. This population consists in:
\begin{itemize}
    \item BBHs that merge within the first 100 Myr, during the $N-$body simulations.
    \item BBHs that will merge within a Hubble time. To calculate them, we consider the population of existing BBHs at 100 Myr and evolve their orbital eccentricity and semi-major axis by integrating the equations of \cite{peters1964}, to calculate the energy loss due to GW emission:
    \begin{eqnarray}
       \frac{{\rm d}a}{{\rm d}t}=-\frac{64}{5}\,{} \frac{G^3 \,{} m_1 \,{} m_2 \,{} (m_1+m_2)}{c^5 \,{} a^3\,{} (1-e^2)^{7/2}}\,{}f_1(e), \nonumber\\
  \frac{{\rm d}e}{{\rm d}t}=-\frac{304}{15}\,{} e \frac{ G^3 \,{} m_1 \,{} m_2 \,{} (m_1+m_2)}{c^5 \,{}a^4 \,{}  (1-e^2)^{5/2}}\,{}f_2(e),\nonumber\\
    \end{eqnarray}
    where
    \begin{eqnarray}
     f_1(e)=\left(1+\frac{73}{24}\,{}e^2+\frac{37}{96}\,{} e^4\right) \nonumber\\
f_2(e)=\left(1+\frac{121}{304} \,{} e^2\right).
    \end{eqnarray}

    All the BBHs that merge within a Hubble time ($t_{\mathrm{H}}= 14 \, \mathrm{Gyr}$) are classified as mergers. This is equivalent to assume that the YSCs dissolve at 100 Myr, and their BBHs evolve only via GW emission (no dynamical interactions) after the death of their parent star clusters.
\end{itemize}
To evaluate how dynamical encounters affect the distribution of BBH mergers in the late phases of the cluster life, we repeat the aforementioned procedure after 1500 Myr, i.e. \begin{itemize}
    \item we count how many BBHs merge within 1500 Myr, during the $N-$body simulations;
    \item we integrate the semi-major axis and eccentricity evolution of the other BBHs that are still bound at 1500 Myr, accounting for GW emission only \citep{peters1964}, and we count how many of them merge within one Hubble time.
\end{itemize}

If the dynamical interactions within the cluster are still effective after 100 Myr, they can affect the population of BBHs, and, consequently, of BBH mergers.
In particular, dynamical processes can form new BBHs or harden the existing ones, allowing them to merge within an Hubble time, or even before the end of the simulation, thus increasing the population of BBH mergers. In some other cases, dynamical interactions can disrupt existing BBHs, possibly removing them from the population of mergers that we estimated at 100 Myr.

\begin{figure*}
\begin{center}
\includegraphics[width=\textwidth]{plots/bbh_dynamical_effect_combined.pdf}
\caption{Mass of the secondary BH ($m_{\mathrm{2}}$) versus the primary BH  ($m_{\mathrm{1}}$) of merging BBHs in low-mass clusters (left) and high-mass clusters (right). Orange diamonds: original BBHs at 1500 Myr. Red crosses: original BBHs at 100 Myr. Light blue circles: exchanged BBHs at 1500 Myr. Blue plusses: exchanged BBHs at 100 Myr. Green circles: exchanged BBHs at 1500 Myr in star clusters with mass $5 \times 10^{4} \, \mathrm{M_{\odot}}$.}\label{fig_bbh_merger}
\end{center}
\end{figure*}

\section{Results}\label{sec_results}

\subsection{Global evolution of the cluster} \label{sec_global}

Figure \ref{fig_radii} shows the evolution of the half-mass radius $r_{\mathrm{h}}$, tidal radius $r_{\mathrm{t}}$, and core radius $r_{\mathrm{c}}$ of the two sets of clusters\footnote{We calculate the half-mass and core radii by considering the whole distribution of stars, not only the bound ones. By this choice, we can easily evaluate when the tidal field affects the relevant scales of the cluster by simply comparing $r_{\mathrm{h}}$ and $r_{\mathrm{c}}$ to $r_{\mathrm{t}}$.}.
Each set is split into three sub-sets of different mass in order to better take into account the impact of the cluster mass on its expansion. As a comparison for high-mass clusters, we also show the evolution of the stellar clusters with $5 \times 10^4 \, \mathrm{M_{\odot}}$.

Low-mass clusters are rapidly disrupted by the tidal field of the host galaxy, as indicated by the steep decrease of the tidal radius. The typical lifetime of these clusters is $400 \, \mathrm{Myr}$, with no particular distinction among the three subsets. As a consequence, $r_{\mathrm{h}}$ steeply increases, and becomes comparable to the tidal radius at about $150 \, \mathrm{Myr}$.
As for the core, its expansion accelerates at about $400 \, \mathrm{Myr}$, when $r_{\mathrm{c}} \sim r_{\mathrm{t}}$ and the tidal effect by the host galaxy disrupts the cluster also at the smallest scales.

High-mass clusters undergo a milder expansion during the first $600-700 \, \mathrm{Myr}$, thanks to their larger initial mass. In this case, the tidal effect of the galaxy becomes significant when $r_{\mathrm{h}} \sim r_{\mathrm{t}}$ and leads to a steeper global expansion.
The decrease of the tidal radius depends on the mass range of the subset, and indicates that the typical lifetime of these systems spans from $1250 \, \mathrm{Myr}$ for clusters below $6000 \, \mathrm{M_{\odot}}$, up to more than $1500 \, \mathrm{Myr}$ for clusters more massive than $7000 \, \mathrm{M_{\odot}}$.
In contrast, the $5 \times 10^4 \, \mathrm{M_{\odot}}$ clusters undergo a far slower expansion and their tidal radius is almost unchanged at the end of the simulation.
As for the core, it undergoes a modest increase throughout the simulation. At the smallest scales, in fact, the effect of the host galaxy becomes important only at the very late stages, suggesting that a bound core is still present at 1500 Myr.

Figure \ref{fig_mfin} shows the distribution of the ratio between the star cluster bound mass at 1500 Myr, $M_{\mathrm{SC,f}}$, and its initial mass, $M_{\mathrm{SC}}$. Low-mass clusters are completely disrupted by the tidal field of the host galaxy at the end of the simulation. In only one case, a dense core of about $120 \, \mathrm{M_{\odot}}$, corresponding to 18\% of the initial mass, can survive, thanks to the presence of a BBH with total mass 80 $\mathrm{M_{\odot}}$.
As for high-mass clusters, one third of the stellar systems is still bound at the end of the simulation. In this set, the number of surviving clusters increases with the initial mass of the cluster. Also, more massive clusters can generally retain a higher fraction of mass. Finally, stellar clusters with $5 \times 10^4 \, \mathrm{M_{\odot}}$ preserve about half of their initial mass at 1500 Myr.

\subsection{BBH populations} \label{sec_bbhl}

Figure \ref{fig_all_bbh} shows the mass distribution of BHs in BBHs at the two considered snapshots: 100 Myr and 1500 Myr. Among the BBH populations, we distinguish between \textit{original BBHs}, whose progenitors were already present as binary stars in the initial conditions of the simulation, and \textit{exchanged BBHs}, which have formed as a consequence of dynamical exchanges.

In low-mass clusters, the BH populations at the two snapshots are almost identical, suggesting that, after $100 \, \mathrm{Myr}$, dynamical encounters play a negligible role in the evolution of BBHs. In contrast, high-mass clusters are still active in producing BBHs at later phases, as indicated by the large increase of exchanged BHs between  $7 \, \mathrm{M_{\odot}}$ and $50 \, \mathrm{M_{\odot}} $.

By comparing the BH populations of the two stellar cluster sets,
we see two main differences. First,
low-mass clusters display a larger number of original BHs with $m_{\mathrm{BH}}> 20 \, \mathrm{M_{\odot}}$. In high-mass clusters, where these BHs undergo strong dynamical interactions, they tend to form exchanged BBHs rather than remain members of original BBHs. Hence, original BBHs in high-mass clusters tend to have lower masses than original BBHs in low-mass clusters.

About 6\% of our simulated BBHs have primary mass $>60 \, \mathrm{M_{\odot}}$. The formation of such massive BHs, with mass ranging from $\sim 60 \, \mathrm{M_{\odot}}$ to $\sim 120 \, \mathrm{M_{\odot}}$ is suppressed in single stellar evolutionary processes by pair-instability (PI) and pulsational pair instability (PPI). Nonetheless, as shown by \cite{spera2018}, \cite{dicarlo2019} and \cite{dicarlo2020}, BHs in the mass gap can form as a consequence of stellar mergers, which produce very massive stars that eventually collapse to BHs. In our simulations, BHs in the PI mass gap form as a result of stellar mergers and generally reside in exchanged systems. However, in 6 cases (5 at 100 Myr),
 a BH with mass $>60$ M$_\odot$ forms in an original binary system. These are systems in which the original binary remains bound after the merger of one component with a third star, producing an original binary with a mass-gap primary BH.

Furthermore, high-mass clusters produce a considerable (about $1.5$ \% of the total) number of BHs with mass $>100 \, \mathrm{M_{\odot}} $, with a maximum mass of $270 \, \mathrm{M_{\odot}} $. In contrast,
only two BHs with mass $>100 \, \mathrm{M_{\odot}} $ form in low-mass clusters. Such intermediate-mass BHs form via multiple stellar collisions \citep{dicarlo2021}.

Figure \ref{fig_bin_form} displays the distribution of formation times of the binary systems that give birth to exchanged BBHs ($t_{\mathrm{form}}$). In low-mass clusters, 8\% of these systems form when  both components are still stars, and about 15\% when one component is a BH.
Most of the BBHs form by the pairing of two BHs, with a peak between $10-20$ Myr. The rapid decrease of the dynamical activity and the dissolution of the stellar cluster cause a steep decrease in the distribution of $t_{\mathrm{form}}$, and only 12\% of the BBHs forms after 100 Myr.

In high-mass clusters, about 88\% of the BBHs form from the pairing of two BHs. In this case, the distribution of $t_{\mathrm{form}}$ shows a flatter trend, hinting at an efficient dynamical activity of the cluster at later times. In this case, in fact, more than one third of the BBHs couple after 100 Myr. In these clusters, only 5\% of BBHs systems form when  both components are still stars.

\begin{comment}

\begin{table}
  \centering
    \begin{tabular}{lrrrr}
    \hline
          & \multicolumn{2}{c}{Low-mass clusters} & \multicolumn{2}{c}{High-mass clusters} \\
          Exch. BBHs & \multicolumn{1}{l}{100 Myr} & \multicolumn{1}{l}{1500 Myr} & \multicolumn{1}{l}{100 Myr} & \multicolumn{1}{l}{1500 Myr} \\
          \hline
          \hline

    $f_{\mathrm{star-star}}$  &  0.78  &  0.78     &  0.26   & 0.21  \\
    $f_{\mathrm{star-BH}}$ &   0.11   &    0.0   &    0.32   & 0.15  \\
    $f_{\mathrm{BH-BH}}$ &  0.11 &   0.22   &  0.41  &  0.64   \\
    \hline
    \end{tabular}
  \caption{ }\label{tab_exch_fractions}
\end{table}%

\end{comment}

\subsection{BBH mergers} \label{sec_mergers}

\subsubsection{Low-mass clusters}

Figure \ref{fig_bbh_merger} shows the mass of the secondary BH ($m_{\mathrm{2}}$) versus the primary BH ($m_{\mathrm{1}}$) for BBH mergers, i.e. BBHs that reach coalescence in less than 14 Gyr.
In low-mass clusters, the population of BBH mergers mostly consists of original BBHs, as a further proof of the poor dynamical activity of these systems. In general, dynamical exchanges do not affect the population of BBHs after 100 Myr (as already suggested by Fig. \ref{fig_all_bbh}), with two exceptions.
First, one BBH that is predicted to merge if the simulation is run only for $100 \, \mathrm{Myr}$, is later disrupted by dynamical interactions, and no longer exists at $1500 \, \mathrm{Myr}$.
Second, the most massive merger (with a final remnant mass $m_{\mathrm{tot}}=99 \, \mathrm{M}_\odot$) needs to dynamically harden for longer than $100 \, \mathrm{Myr}$ to enter the regime in which the orbital decay by GWs becomes effective. As shown in Fig. \ref{fig_bin_form} (bottom panel), 75\% of the merging BBHs form at  early stages, when  both components are stars. At later stages, the scarce efficiency of dynamical hardening in low-mass clusters quenches the formation of further BBH mergers.

The properties of BBH mergers are summarized in Table~\ref{tab_BBHmergers}.
In low-mass clusters, all the BBHs are no longer bound to their host cluster when they merge.
In this work, a BBH merger is labelled as bound to the cluster if it merges inside the cluster during the simulation, or (if it has not merged during the simulation) is still bound to the cluster at $1500 \, \mathrm{Myr}$.

\begin{table}
  \centering
    \begin{tabular}{lrrrr}
    \hline
          & \multicolumn{2}{c}{Low-mass clusters} & \multicolumn{2}{c}{High-mass clusters} \\
          BBH mergers & \multicolumn{1}{l}{100 Myr} & \multicolumn{1}{l}{1500 Myr} & \multicolumn{1}{l}{100 Myr} & \multicolumn{1}{l}{1500 Myr} \\
          \hline
          \hline

    All  &  35     &  35     &  97   & 115  \\
    Original &   27    &    27   &    63   & 54  \\
    Exchanged &  8     &    8   &  34  &  61  \\
    Inside YSC  &    0   &   0    &   13    &  5  \\
    IMBHs  &    0   &   0    &  1    &  6  \\
    $m_{\mathrm{tot, max}} \, [\mathrm{M_{\odot}}]$   &    58   &   99    &  116    &  158  \\
    \hline
    \end{tabular}
  \caption{We report the number of all (first row), original (second row) and exchanged (third row) BBH mergers. We also show the number of BBHs that either merge inside the cluster or are still bound to the cluster at the end of the simulation and merge within one Hubble time (fourth row). Finally, we report the number of IMBHs produced by BBH mergers (merger remnants, fifth row), and their maximum BH mass (last row).
  }\label{tab_BBHmergers}
\end{table}%

\subsubsection{High-mass clusters}
High-mass star clusters host a population of BBH mergers about three times larger than low-mass clusters, although the total initial stellar masses of the simulated star cluster samples are approximately the same.
This enhancement of BBH mergers in high-mass clusters is particularly evident for the exchanged systems, which, at $1500 \ \mathrm{Myr}$, represent the majority of BBH mergers.

The populations of BBH mergers at 100 and 1500 Myr show notable differences.
A number of original BBHs that are predicted to merge at 100 Myr are later disrupted (Figure \ref{fig_bbh_merger} and Table~\ref{tab_BBHmergers}).
Some exchanged BBHs are also disrupted after the first $100 \, \mathrm{Myr}$. However, these disrupted exchanged BBHs are compensated by the  late formation and/or hardening of other exchanged BBHs: we predict only 34 merging exchanged BBHs at 100 Myr, while at 1500 Myr we find 61 merging exchanged BBHs, as shown in Table~\ref{tab_BBHmergers}.
As a result, at $1500 \, \mathrm{Myr}$, the number of exchanged BBH mergers has increased by a factor of two with respect to $100$ Myr. As shown in Fig. \ref{fig_bin_form}, most of the merging BBHs at 1500 Myr form when  both components have already evolved to BHs. As opposed to low-mass clusters, merging BBHs can form at very late stages, up to $1000 $ Myr.
In high-mass clusters, six BBH mergers give birth to intermediate mass black holes (with a remnant mass $m_{\mathrm{tot}}> 100 \, \mathrm{M_{\odot}}$). In the two most massive mergers, the primary BH is itself an IMBH. The most massive remnant has a total mass $m_{\mathrm{tot}}=158 \, \mathrm{M_\odot}$.

Figure \ref{fig_chirp} shows the distribution of chirp masses of merging BBHs, for the two snapshots considered. The changes in the distribution are mostly due to the long-term dynamical activity within high-mass clusters. Late dynamical activity triggers a large increase of the number of mergers with high chirp mass $m_{\rm chirp}\approx 35 \, \mathrm{M_{\odot}}$.

\subsection{BBH orbital properties at formation}

To estimate for how long a stellar cluster is dynamically active and can affect the formation of BBH mergers, we evaluated $t_{\mathrm{M}}$, defined as the time (since the beginning of the simulation) at which the semi-major axis of the BBH has become sufficiently tight to merge within a Hubble time via GW emission.
Figure \ref{fig_a0_e0} shows $t_{\mathrm{M}}$ as a function of the orbital properties of the BBH when it forms, that is its semi-major axis ($a_{\mathrm{BBH}}$) and its orbital eccentricity ($e_{\mathrm{BBH}}$).

\begin{figure}
\begin{center}
\includegraphics[width=\hsize]{plots/chirp_mass_histograms_single.pdf}
\caption{Chirp mass distribution at 100 Myr (light-blue filled histogram) and at 15000 Myr (blue line), for all the simulated clusters.}\label{fig_chirp}
\end{center}
\end{figure}

\begin{figure*}
\begin{center}
\includegraphics[width=\textwidth]{plots/bbh_a0_tpet_e0_combined.pdf}
\caption
Time at which the semi-major axis of the BBH has become sufficiently tight to merge within a Hubble time via GW emission (according to \protect{\citealt{peters1964}}) versus semi-major axis of the BBH when it forms ($a_{\mathrm{BBH}}$), for merging BBHs in low-mass clusters (left) and high-mass clusters (right). The markers are the same as in Figure \ref{fig_bbh_merger}. The colour-map encodes the information on the orbital eccentricity at the BBH formation, $e_{\mathrm{BBH}}$. If a BBH at 1500 Myr is also present at 100 Myr, it is marked with a white cross (original) or plus (exchanged).}\label{fig_a0_e0}
\end{center}
\end{figure*}

\begin{figure*}
\begin{center}
\includegraphics[width=\textwidth]{plots/bbh_mtot_tpet_tBBH_combined.pdf}
\caption
Time at which the semi-major axis of the BBH has become sufficiently tight to merge within a Hubble time via GW emission (according to \protect{\citealt{peters1964}}) versus total mass of the BBH merger ($m_{\mathrm{tot}}$), for merging BBHs in low-mass clusters (left) and high-mass clusters (right). The markers are the same as in Figure \ref{fig_bbh_merger}. The colour-map encodes the information on the time at which the BBH forms, $t_{\mathrm{BBH}}$. If a BBH at 1500 Myr is also present at 100 Myr, it is marked with a white cross (original) or plus (exchanged).}\label{fig_mtot_tM}
\end{center}
\end{figure*}

In both low-mass and high-mass clusters, the original BBH mergers show typical values of $t_{\mathrm{M}} \lesssim 10 \, \mathrm{Myr}$,  $a_{\mathrm{BBH}} \lesssim 0.1 \, \mathrm{AU}$, and circular orbits. These properties spring from their formation pathway. These BBHs are, in fact, the result of original binaries that hardened as a consequence of a common envelope phase. When the second BH forms, the orbital properties of the BBH already allow it to merge within an Hubble time. For this class of BBH mergers, then, $t_{\mathrm{M}}$ mainly coincides with the time at which the second BH in the binary forms. Also, because the common envelope phase leads to a large mass loss, the resulting BH masses are systematically smaller than the exchanged ones.

As a confirmation of this idea,
Fig. \ref{fig_mtot_tM} shows $t_{\mathrm{M}}$ as a function of the total mass of the merging BBH, $m_{\mathrm{tot}}$ and the time at which the BBH forms, $t_{\mathrm{BBH}}$. Original BBHs have  $t_{\mathrm{BBH}}\lesssim 10 \,{\mathrm{Myr}}$ and, in most cases, $t_{\mathrm{BBH}}=t_{\mathrm{M}}$. In high-mass stellar cluster, one original BBH presents $t_{\mathrm{M}}>t_{\mathrm{BBH}}$: in this case, dynamical hardening allows the binary system to enter the merging regime after the BBH formation.
In contrast, $t_{\mathrm{BBH}}$ ranges from 5 Myr to 1000 Myr for exchanged BBHs. In high-mass clusters, 13 BBHs form after the first 100 Myr. Because exchanged BBHs have not undergone mass loss by a common envelope phase, their masses are systematically higher than those of original BBH mergers, with $m_{\mathrm{tot}} \gtrsim 40 \, \mathrm{M_{\odot}}$.

In low-mass YSCs, only three exchanged BBH mergers have
$a_{\mathrm{BBH}} \gtrsim 0.1$ AU. In two cases, these mergers correspond to the two most massive BBHs, which formed in dynamically active environments. As a further proof of their dynamical origin, these BBHs are characterized by eccentric orbits.
In high-mass clusters, where dynamical interactions play a major role, the distribution of BBH mergers extends to higher values of $a_{\mathrm{BBH}}$ and $t_{\mathrm{M}}$.
In particular, exchanged binaries, when they form, are generally characterized by large  semi-major axes, up to $5\times10^{4} \, \mathrm{AU}$, and thus take longer times to enter the regime in which GWs efficiently shrink the semi-major axis. In some cases, $t_{\mathrm{M}}$ can be as high as $1400 \, \mathrm{Myr}$, indicating that dynamical hardening can play a role even at the very end of the simulation.

Finally, the dynamical encounters that lead to the formation of BBHs
leave a
distinctive imprint on their eccentricity. The resulting binary systems are, in fact, characterized by larger eccentricities at formation, with $e_{\mathrm{BBH}}>0.1$. Exchanged BBHs that have values of $t_{\mathrm{M}} \lesssim 100 \, \mathrm{Myr}$ and high eccentricities can be later disrupted by dynamical interactions, and are no longer present at 1500 Myr.

\subsection{Formation pathway of black holes in the mass gap}

In high-mass stellar clusters, $5$ BBH mergers
have primary mass in the PI mass gap.
As mentioned in Section \ref{sec_bbhl}, such massive objects originate from the merger of massive stars.
Figure \ref{fig_PI} shows the evolution of BHs in BBH mergers in the PI mass gap. In all cases, the progenitor star undergoes at least one merger with another star. The merger product of such stellar collisions is an exotic star, with an undersized He core with respect to the hydrogen-rich envelope. Such  star does not develop PI, because its central properties (temperature and density) do not fall within the PI regime \citep[e.g.,][]{renzo2020b,costa2021}. At the end of its evolution, the stellar product directly collapses into a BH more massive than $60 \, \mathrm{M_{\odot}}$.

Successive mergers between the BH and non-compact objects do not affect the mass of the BH because, consistently with \cite{dicarlo2020,dicarlo2020b}, we assume that the short timescale of the merger does not allow the BH to accrete mass (but see \citealt{rizzuto2021} for a different assumption). In all the BBH mergers, the binary system forms when both objects are BHs. In one case, the BBH is disrupted by dynamical interaction at 105 Myr.

\begin{figure}
\begin{center}
\includegraphics[width=\hsize]{plots/binary_core_PI_ALL.pdf}
\caption{Evolution of the total mass (thick lines) and the core
mass (thin lines) of the progenitors of the BHs
in the PI mass gap. Dashed lines mark the time interval before the star becomes a BH.
Different markers indicate: the merger between the progenitor star or the BH and another star (stars), the time when the BBH is formed (open circles), and the time at which the binary is possibly disrupted (crosses).}\label{fig_PI}
\end{center}
\end{figure}

\section{Summary} \label{sec_conclusions}

We have studied the formation of BBHs in young and open star clusters via direct $N$-body simulations, exploiting the codes {\sc nbody6++GPU} \citep{wang2015} and {\sc mobse} \citep{mapelli2017}.  We simulated two different classes of star clusters: low-mass (500--800 M$_\odot$) and high-mass (5000--8000 M$_\odot$) systems. We find that the properties and timescales of BBH mergers in the two  star-cluster families are extremely different.

In low-mass clusters, most BBHs form in the first 100 Myr and are the result of the evolution of original binary stars,
which evolve through common envelope. They do not harden significantly after $\sim{100}$ Myr.
In contrast, the late evolutionary stages ($>1$ Gyr) are crucial for high-mass clusters. Exchanged BBHs (i.e., BBHs that form via dynamical exchanges) are the most common BBH mergers in high-mass clusters (Figures~\ref{fig_all_bbh} and \ref{fig_bbh_merger}). While exchanged BBHs form preferentially in the first $\sim{100}$~Myr, they keep hardening significantly until the end of the simulations (1.5 Gyr, Figure~\ref{fig_bin_form}). This confirms the importance of integrating the evolution of relatively massive clusters ($\gtrsim{}5000$ M$_\odot$) for $>1$ Gyr,

This difference between the BBH population of low-mass and high-mass star clusters mostly springs from the different two-body relaxation timescale and tidal disruption timescale of the two star cluster families. Our low-mass and high-mass star clusters have a
two-body relaxation timescale \citep{spitzer1987} of $\sim{10}$ Myr and $\sim{30}$ Myr, respectively.
This means that mass segregation and other dynamical processes happen earlier in low-mass clusters. Furthermore, low-mass clusters become tidally overfilling already at $\sim{150}$ Myr, while the half-mass radius of our high-mass clusters becomes comparable to the tidal radius only at $\sim{500}$ Myr (Figure~\ref{fig_radii}). Hence, the dynamical activity of the low-mass clusters is quenched by tidal evaporation about five times earlier than that of high-mass clusters.

In both low-mass and high-mass clusters, the latest BBHs that form (exchanged BBHs) are the most massive ones (primary mass $\gtrsim{}30$ M$_\odot$), because dynamical exchanges favour the pairing of the most massive BHs (Figure~\ref{fig_bbh_merger}). The distribution of the chirp mass of BBH mergers shows two main peaks: the first  at $\sim{7-15}$ M$_\odot$ and the second at $\sim{30-40}$ M$_\odot$. However, the high-mass peak develops only
after 100 Myr (Figure~\ref{fig_chirp}).

BBH mergers in low-mass clusters are driven mostly by binary evolution via common envelope: they form with short semi-major axis ($\sim{0.1}$~AU) and low orbital eccentricity (Figure~\ref{fig_a0_e0}). In contrast, massive BBHs in high-mass clusters form with larger semi-major axis ($>10$~AU) and higher orbital eccentricity ($0.1-1$).

A non-negligible percentage ($4\%$) of our simulated BBH mergers in high-mass clusters have primary component's mass in the pair-instability (PI) mass gap. All of them form via stellar collisions, in which a main-sequence star merges with a more evolved star (core He burning). About 40\% of these massive BBHs leave a merger remnant in the intermediate-mass BH range. In contrast, we find no IMBHs in the low-mass clusters.

Furthermore, in the high-mass clusters, we find a few original BBHs with primary mass in the PI mass gap. These are  systems in which one of the two components of the binary star undergoes a collision with a third star and collapses to a BH in the PI mass gap without leading to the ionization of the original binary system.

Overall, our study shows that the formation channels of BBHs in low-mass ($\sim{500-800}$ M$_\odot$) and high-mass star clusters ($\ge{5000}$ M$_\odot$) are extremely different and lead to two completely distinct BBH populations. Low-mass clusters host mainly low-mass BBHs born from binary evolution, while BBHs in high-mass clusters are relatively massive and driven by exchanges. This difference is crucial for the interpretation of gravitational-wave sources.

\section*{Acknowledgements}

MM, AB and SR knowledge financial support from the EuropeanResearch Council for the ERC Consolidator grant DEMOBLACK, under contract no. 770017.
We thank Nicola Giacobbo and the members of the DEMOBLACK team for useful discussions. We acknowledge that the results of this research have been achieved using the DECI resource Snellius based in the Netherlands at SURFsara, with
support from the PRACE aisbl.
MP acknowledges financial support from the European Union's Horizon 2020 research and innovation programme under the Marie Sklodowska-Curie grant agreement No. $896248$. ST thanks Mark Gieles and the ICCUB Virgo team for useful comments and discussions.

\section*{Data availability}
The data underlying this article will be shared on reasonable request to the corresponding authors.  The latest public version of {\sc mobse} can be downloaded from \href{https://gitlab.com/micmap/mobse_open}{this repository}.

\begin{comment}
\begin{figure*}
\begin{center}
\includegraphics[width=\textwidth]{plots/bbh_tpeters_combined.pdf}
\caption{Mass of the secondary BH ($m_{\mathrm{2}}$) versus mass of the primary BH ($m_{\mathrm{1}}$) for merging BBHs in low-mass clusters (left) and high-mass clusters (right). The symbol prescription is the same as Fig. \ref{fig_bbh_merger}. The colormap encodes the information on $t_{\mathrm{P}}$. If a BBH at 1500 Myr is also present at 100 Myr, it is marked with a white cross (original) or plus (exchanged).\ST{Questa immagine alla fine mi sembra di troppo, non la metterei.}}\label{fig_tP}
\end{center}
\end{figure*}

\end{comment}

\bibliographystyle{mnras}

redpajama_set_name: RedPajamaArXiv


text: One web program built with django.

redpajama_set_name: RedPajamaGithub


Suffering From A Job Related Casualty in Dickinson Texas?
Seek Accident at Work Related Lawyers From Hildebrand & Wilson, LLP For Help!
Frequently personnel are injured at a job site because accidents do happen. In most cases, employers have workers comp coverage to compensate for the doctors bills and missing pay their staff have sustained.
So what occurs if your business does not carry employers liability insurance?
Try to get help from financial assistance?
No - you ought to obtain the assistance of Accident at Work Related Lawyers in Dickinson Texas with Hildebrand & Wilson, LLP! They are experienced and trained to help staff injured at a work site whose employer doesn't carry workers comp coverage.
Just what could the Accident at Work Related Lawyers at Hildebrand & Wilson, LLP handle for your construction claim for injuries?
File a lawsuit if needed against your business owner!
If medical bills are multiplying and you are unable to perform your job duties as a consequence of trauma acquired in a worksite unfortunate occurrence, you should get assistance! Rely on the Accident at Work Related Lawyers in Dickinson Texas from Hildebrand & Wilson, LLP. Do not be in pain from personal trauma you got at a workplace – seek help without any further delay!


November 23, 2018 (KHARTOUM) - The UN Resident and Humanitarian Coordinator for Sudan, Gwi-Yeop Son, on Thursday has discussed with the governor of South Kordofan State Ahmed Mufadal ways to deliver humanitarian assistance to rebel-controlled areas.
In a press statement to the official news agency SUNA, Mufadal said the meeting discussed the Sudan People's Liberation Movement/North (SPLM-N) stance towards allowing access to humanitarian aid to areas under its control.
He demanded the UN agencies to put more pressure on the SPLM-N to allow the delivery of humanitarian aid to the needy population, renewing the government position in this regard.
Mufadal added the meeting also discussed the importance of coordination between the government and the UN to deliver the humanitarian aid to the needy, stressing the security situation in South Kordofan is calm and stable.
For her part, the UN official said she came to South Kordofan to learn about services rendered by aid and development groups in the state.
She pointed to the need to enhance cooperation with the government to promote humanitarian and development work and reduce the poverty rate in order to achieve peace in South Kordofan.
The Sudanese army has been fighting the SPLM-N rebels in the Blue Nile and South Kordofan, also known as the Two Areas since 2011.
Last September, Sudan agreed to an initiative from the UN to deliver humanitarian assistance to civilians in the rebel-controlled areas in the Blue Nile and South Kordofan states.
The details of the UN initiative are made public but they seem similar to a former plan prepared b a tripartite committee including UN, African Union and the Arab League providing that the humanitarian assistance will be delivered from Sudan after its control by the Sudanese authorities and its distribution will be monitored by UN, AU and Arab observers to ensure that the rebels will not get it.
The SPLM-N officials in the past told the mediation they insist on the external stations because they want to have a humanitarian corridor to ensure the transportation from the landlocked rebel-areas of ill or wounded fighters to outside the country for treatment.
Also, during the last round of talks from 1 to 3 February 2018, the Sudanese government and SPLM-N al-Hilu failed to reach a cessation of hostilities agreement. The rebel faction which controls the Nuba Mountains areas now wants all the humanitarian assistance to be delivered from outside Sudan.


text:
//go:build linux || darwin
// +build linux darwin

package fs

import (
	"context"
	"encoding/base64"
	"strings"
	"sync"

	"perkeep.org/pkg/blob"
	"perkeep.org/pkg/schema"
	"perkeep.org/pkg/search"

	"bazil.org/fuse"
)

// xattrPrefix is the permanode attribute prefix used for record
// extended attributes.
const xattrPrefix = "xattr:"

// xattr provides common support for extended attributes for various
// file and directory implementations (fuse.Node) within the FUSE services.
type xattr struct {
	typeName  string // for logging
	fs        *CamliFileSystem
	permanode blob.Ref

	// mu guards xattrs.  Both mu and the xattrs map are provided by the
	// fuse.Node when the struct is created.
	mu *sync.Mutex

	// This is a pointer to the particular fuse.Node's location of its
	// xattr map so that it can be initialized commonly when the fuse.Node
	// calls xattr.load(*search.DescribedPermanode)
	xattrs *map[string][]byte
}

// load is invoked after the creation of a fuse.Node that may contain extended
// attributes.  This creates the node's xattr map as well as fills it with any
// extended attributes found in the permanode's claims.
func (x *xattr) load(p *search.DescribedPermanode) {
	x.mu.Lock()
	defer x.mu.Unlock()

	*x.xattrs = map[string][]byte{}
	for k, v := range p.Attr {
		if strings.HasPrefix(k, xattrPrefix) {
			name := k[len(xattrPrefix):]
			val, err := base64.StdEncoding.DecodeString(v[0])
			if err != nil {
				Logger.Printf("Base64 decoding error on attribute %v: %v", name, err)
				continue
			}
			(*x.xattrs)[name] = val
		}
	}
}

func (x *xattr) set(ctx context.Context, req *fuse.SetxattrRequest) error {
	Logger.Printf("%s.setxattr(%q) -> %q", x.typeName, req.Name, req.Xattr)

	claim := schema.NewSetAttributeClaim(x.permanode, xattrPrefix+req.Name,
		base64.StdEncoding.EncodeToString(req.Xattr))
	_, err := x.fs.client.UploadAndSignBlob(ctx, claim)
	if err != nil {
		Logger.Printf("Error setting xattr: %v", err)
		return handleEIOorEINTR(err)
	}

	val := make([]byte, len(req.Xattr))
	copy(val, req.Xattr)
	x.mu.Lock()
	(*x.xattrs)[req.Name] = val
	x.mu.Unlock()

	return nil
}

func (x *xattr) remove(ctx context.Context, req *fuse.RemovexattrRequest) error {
	Logger.Printf("%s.Removexattr(%q)", x.typeName, req.Name)

	claim := schema.NewDelAttributeClaim(x.permanode, xattrPrefix+req.Name, "")
	_, err := x.fs.client.UploadAndSignBlob(ctx, claim)

	if err != nil {
		Logger.Printf("Error removing xattr: %v", err)
		return handleEIOorEINTR(err)
	}

	x.mu.Lock()
	delete(*x.xattrs, req.Name)
	x.mu.Unlock()

	return nil
}

func (x *xattr) get(req *fuse.GetxattrRequest, res *fuse.GetxattrResponse) error {
	x.mu.Lock()
	defer x.mu.Unlock()

	val, found := (*x.xattrs)[req.Name]

	if !found {
		return fuse.ErrNoXattr
	}

	res.Xattr = val

	return nil
}

func (x *xattr) list(req *fuse.ListxattrRequest, res *fuse.ListxattrResponse) error {
	x.mu.Lock()
	defer x.mu.Unlock()

	for k := range *x.xattrs {
		res.Xattr = append(res.Xattr, k...)
		res.Xattr = append(res.Xattr, '\x00')
	}
	return nil
}


Rising third graders start summer school today. The five-week sessions are held at every elementary school in the district, running from June 22 – July 2 and August 3 – 20, from 9 a.m. until noon. Breakfast and lunch are offered at every site.
This is the second year of the program and, according to Donovan, last year's fall assessments for participating students showed their reading and math skills stayed strong over the summer.
"Part of our goal is to reduce the summer regression for literacy and math," said Donovan.


text:
The gospel according to Paglia
By Cathal KellySports Columnist
Camille Paglia is speaking on the phone from her home in Philadelphia. Ten minutes into the verbal torrent, she stops and asks, "Are you taping this?"
"Oh good, I can talk faster."
And then, unbelievably, she does.
Talking to Paglia is like showering under Niagara Falls. The only goal is to stay upright.
The academic, culture critic and professional contrarian is 62 now. But her oft-noted intensity burns as brightly as ever. Paglia wants to talk to you, to explain things to you, and, if you are foolish enough to disagree, to utterly destroy you.
On Tuesday, Paglia will be the third and final speaker at the Royal Ontario Museum lecture series entitled The Three New Commandments.
Of course, Paglia being Paglia, she's already changed the terms of her address. She's not interested in three new commandments. Instead, she will meld two of her pre-eminent concerns – Hollywood and the Bible.
There will be an audio-visual component. "We'll be showing some segments from a movie," she says.
Which movie?
"I won't reveal which."
It wouldn't be The Ten Commandments, would it?
"Oh, alright, you've guessed it! Ha, ha, ha!" Paglia says, sounding more excited than anyone has a right to be at 10 a.m.
Paglia is a hypnotic speaker, weaving together disparate threads from arcane to Archie. She manages to explain the grip of post-structuralism on Western thought with an analogy to Lily Tomlin's dream sequence in Nine to Five. On Tuesday, she plans to work without a script.
"I don't know what I'm going to say. But I have to feel it. I have tons to talk about."
That being the case, those planning to attend may want to bring their audio recorders and a flask of coffee. "Is there a point when they have to clear the room?" Paglia asks ominously. "My dream would be to go on for hours. The damn movie is three hours long."
Paglia was raised a Catholic by Italian immigrant parents in upstate New York. She admired – and still does – the ritual, the connection to classical learning and history. She chafed at the rigidity.
Her break from Catholicism had three seminal moments – each one partially explaining one of Paglia's obsessions.
The first was spotting Elia Kazan's film Baby Doll on a list of "condemned"' movies posted by the now-defunct Legion of Decency in her church. The second was asking a nun if, since God was all forgiving, he would ever forgive Satan. The answer – inarticulate rage – convinced her that the church "has no place for an inquiring mind." The third was reading Corliss Lamont's 1935 investigation of life after death, The Illusion of Immortality.
Nevertheless, Paglia is a great friend of the Bible, and of religious experience in general.
"I don't believe it's the word of God," Paglia says. "I believe it's inspired poetry. What worries me is that with our tilt toward secularism, I'm discovering how distant young people have become from the Bible. The unintended consequence of this is that most liberal young people are losing the ability to understand Western art."
As a tonic, Paglia has long proposed that a course in comparative religion be a cornerstone in American schools.
This all sounds quite collegial. But the truest, most appealing face Paglia wears is that of a pugnacious and tireless enemy. No opportunity to kick her foes, living or dead (e.g. philosophers Jacques Derrida, Michel Foucault and Martha Nussbaum, and journalist Susan Faludi), can be allowed to pass.
The tangent on teaching leads inevitably to another of her bugbears: conventional pedagogic wisdom.
"The true multiculturalism is comparative religion," she says. "Not teaching some victim-oriented, genocide-laden kinds of history – the way multiculturalism is ordinarily taught is through victims. (Voice dipping to a low whine) Oh, the Spanish came and committed genocide. Christopher Columbus was guilty of genocide. All of that."
She doesn't do debates anymore, an enormous shame however one feels about her views. Anyone who saw her vivisect Faludi in an iconic episode of The Phil Donahue Show 17 years ago knows exactly how enormous.
"Debate who? On what? Who would I debate?" Paglia cries, faux-appalled.
Arch-atheist and essayist Christopher Hitchens for a start. Nearly two weeks ago, Hitchens was the first speaker in this ROM-sponsored series. Maybe he can be recalled for a championship tilt with Paglia to close the show.
"Hitchens is a cynic and he knows nothing about religion," Paglia starts out, slowly punctuating each word – a sure sign of danger. "It's one thing to attack it from the basis of knowledge... I thought that book (Hitchens' God Is Not Great) was awful. Awful book! That could have been a great book ... He's, like, lazy. He's lazy! He just wants to sit around and have dinner parties and drink in Washington. The whole book is, like, chatted. (High, mocking tone) And then I was with a Muslim guy in a taxi with my wife ... C'mon. What is that? It's not even a magazine article ... I think it's a scandal."
Paglia has taught at the Philadelphia College of Performing Arts for a quarter-century. She contributes a regular column to Salon.com. She's also working on the follow-up to her compendium of great poems, Break Blow Burn. The next tome – her books are always big enough to double as bludgeons – will provide an introduction to visual arts. There's no release date in sight. In direct opposition to her manner of speaking, Paglia writes with what she calls "painful slowness.
"Oh Lord, when will it be done! As Rex Harrison as the Pope said to Charlton Heston as Michelangelo (in The Agony and the Ecstasy) – ha, ha! – `When will you be done?'" Paglia cackles.
"But unlike Christopher Hitchens, I take books seriously."
Camille Paglia speaks Tuesday at the ROM's Dead Sea Scrolls Director's Signature Series (www.rom.on.ca/scrolls).

redpajama_set_name: RedPajamaCommonCrawl


Subject grew up in eastern Long Island and was living in Yonkers (just north of Manhattan) at the time of this interview.
Subject speaks carefully and precisely and with a love of words. She is a good model for higher socio-economic characters.


text:
National Cheat Sheet: US home sales drop again, JLL acquires HFF for $2B… & more
TRD New York /
Mar.March 22, 2019 08:00 AM
Clockwise from top left: The Federal Reserve has held interest rates steady and indicated that they will not rise this year; Facebook revamps its housing ad policy after settling discrimination lawsuits; JLL buys HFF in a $2B cash-and-stock deal that it hopes will 'accelerate growth;' and a Re/Max report finds the U.S. set for a 'significant shift' as home sales decline and inventory grows.
Report: 'Shift' as US home sales decline, inventory grows
U.S. home sales continued to fall in February, dropping 4.2 percent, even as inventory grew by 5.8 percent, according to a new report from Re/Max. The decrease in home sales marked the seventh consecutive month of declines year-over-year, although the increase in inventory was the fifth month in a row of growth, the report said. Trends that last five months or more "often indicate significant shifts," said a statement from Re/Max CEO Adam Contos. "Year-over-year trends in declining sales and rising inventory have both reached that length now," he added. Homes in San Francisco and Omaha, Nebraska, were on the market for the least amount of time at 37 and 34 days, respectively, according to the report. [TRD]
JLL buys HFF for $2B in effort to 'accelerate growth'
Chicago-based JLL announced this week a $2 billion cash-and-stock deal to acquire Dallas-based HFF. The proposed combination, which could usher in a period of poaching as rival commercial brokerages seek to attract individuals displaced by the union, values HFF at $49.16 per share based on its March 18 market closing price. The merger, which should be finalized in the third quarter of this year, still requires HFF shareholder approval, but already has the assent of both companies' boards. "The combination with HFF provides a unique opportunity to accelerate growth and establish JLL as a leading capital markets intermediary, with outstanding capabilities," said a statement from JLL global CEO Christian Ulbrich. JLL and HFF are both in the top 10 in The Real Deal's recent ranking of investment sales firms. [TRD]
Opendoor valuation hits $3.8B after funding round
San Francisco-based startup Opendoor, which has sought to make a name for itself in the iBuyer space, has raised $300 million in a funding round led by General Atlantic, Fifth Wall Ventures, GGV Capital, Hawk Equity and Japan's SoftBank Group, according to TechCrunch. The outlet noted the move brings Opendoor's valuation to $3.8 billion. Founded in 2014, Opendoor has since raised $1.3 billion in equity, with another $3 billion in debt financing to purchase properties. The company, which received a $400 million investment from SoftBank late last year, plans to use its latest round of funding on product development and expansion. Opendoor co-founder Eric Wu told TechCrunch that his company intends to remain focused on the private home buying market, rather than cars, commercial real estate or loans. [TRD]
Facebook settles lawsuits, revamps housing ad policy
Online housing advertisements will no longer target Facebook users by ZIP code, the Wall Street Journal reported. A new policy enacted by the social media giant will also set a 15-mile minimum radius for geographic ads and restrict housing, job and lending ads from targeting users by age and gender. Facebook is making the changes to settle five discrimination lawsuits filed by plaintiffs, including the National Fair Housing Alliance. "There is a long history of discrimination in the areas of housing, employment and credit, and this harmful behavior should not happen through Facebook ads," company COO Sheryl Sandberg wrote in a blog post. [TRD]
Fed holds interest rates, indicates no raises this year
The Federal Reserve isn't raising interest rates right now, and will most likely hold them steady for the rest of the year due to concerns about an economic slowdown. In 2018, the Fed raised rates four times. In minutes this week, officials indicated that 2020 will only see one rate raise. The decision reflects a relatively recent change of mind on behalf of top Fed officials. At the end of last year, only two two officials said they thought the Fed would keep interest rates unchanged in 2019, as opposed to 11 out of 17 right now. The Fed also plans to scale back its plan to downsize its portfolio of government-backed securities. Low interest rates have been a boon to real estate investment trusts and could lead to more demand for mortgages from Freddie Mac, a government-sponsored entity that the Trump administration is considering privatizing. This week Freddie Mac promoted president David Brickman to CEO. [TRD]
MAJOR MARKET HIGHLIGHTS
Manhattan's Hudson Yards development officially opens
A star-studded extravaganza of business moguls, celebrities, developers, elected officials and even Big Bird turned out last week to celebrate the grand opening of Hudson Yards on Manhattan's West Side — first at an invite-only evening soiree on March 14 and again at a ceremony the next morning. New York Sen. Chuck Schumer called Related Companies chairman Stephen Ross the "only person in the universe" who could have brought the decade-long development to fruition. Ross, meanwhile, said he was "still awed" to see the project become a reality. Since the opening, critics have raised concerns about Related's use of surveillance in the neighborhood, as well as its controversial policy regarding photos taken from a 15-story climbable sculpture known as "The Vessel." [TRD]
Boston, LA touted as top cities to endure economic downturn
Among the cities that could remain among the most resilient amid the country's economic slowdown is Boston, one of several places that investors have set their sights on that are less likely to feel the effects of a downturn, Bloomberg reported. Boston is considered a less riskier investment because it has a traditional financial services base, as well as a biotechnology and life sciences sector, according to the outlet. Los Angeles is another city that's drawing in investors due to its media and technology industries. Cities such as Austin, Texas, which rely predominantly on a single industry or company, are considered riskier places to invest. [TRD]
ISG founders resolve acrimonious partnership dispute
Two founders of Miami-based luxury brokerage International Sales Group have officially parted ways after settling dueling lawsuits last month. Philip Spiegelman had accused Craig Studnicky of mismanaging "large amounts of cash," while Studnicky had claimed Spiegelman pushed out a third founding partner of ISG and alienated clients with his "overbearing narcissism and obnoxious personality." The litigation initially left the future of the brokerage up in the air, but Studnicky's lawyer Robert Stok said the two have "reached an amicable resolution." Stok's client will take over ISG, while Spiegelman will get development rights to a mixed-use project in New Orleans. [TRD]
Michigan nonprofit moves into OZs in Florida
The Troy, Michigan-based Kresge Foundation is the latest entrant in the race to reap the benefits from federal Opportunity Zones. The philanthropic group, a registered nonprofit, has partnered with Boston-based Arctaris Impact and Fort Lauderdale-based Community Capital Management to launch an OZ-focused fund. Kresge has provided a combined $22 million to both funds, which have agreed to adhere to certain investment guidelines, such as deploying capital to create jobs and help low-income communities. OZs allow investors to defer paying capital gains taxes if they invest in specially designated geographic areas. U.S. Housing and Urban Development Secretary Ben Carson told The Real Deal earlier this month that he would give preferential treatment to OZ developers and investors that build affordable housing. [TRD]
PMG to bring another co-living complex to Chicago
Property Markets Group plans to open another co-living rental complex in Chicago, principal Noah Gottlieb told The Real Deal. The New York-based developer, which started its co-living unit in 2017, has already opened two "X Social Communities" complexes in the Windy City and one complex in Miami. New apartment buildings are in the works in Denver, Oakland, Phoenix and several cities in Florida, and the group is eyeing Atlanta, Houston and Minneapolis for future projects, Gottlieb said. Beds start at $995 per month in PMG's "X Chicago" building in the University Village neighborhood. [TRD]
Santa Monica's Clock Tower Building sells for $58M
Sorgente Group of America has sold the historic Clock Tower Building in Santa Monica to Rockwood Capital for $58 million. The 53,500-square-foot Art Deco tower, which opened in 1930, was the tallest building in the beachfront city for four decades. It's considered Santa Monica's first skyscraper and is also still one of the tallest buildings in the vicinity due to height restrictions. The building, which has a four-story clock tower, is currently home to Chinese digital media company Hylink, investment firm Bold Capital Partners and H Code media, among other tenants. Italy's Sorgente Group, whose other properties include the Flatiron Building in Manhattan, bought the Clock Tower Building in 2013 for around $34 million. [TRD]
facebookfederal reservehffHudson YardsJLLopendoorRe/max
Hudson Yards megadevelopment inspires a new line of sex toys
Views from 1,100 feet: A tour of Related's "the edge," the tallest outdoor observation deck in the Western Hemisphere
Facebook close to finalizing Hudson Yards office deal: report
L3's Williamsburg retail properties snag $91M refi
Related's CEO talks Hudson Yards and "complicated" projects
Triple-digit office rents, once a rarity, are now a major piece of Manhattan deals
Market value of NYC real estate went up at slowest rate in years
Related drops 700-foot-long "wall" from Hudson Yards plan


Those of us who happened to be born into a Christian family or environment, most likely have already received sacramental or sanctifying "grace," as an infant, through the sacrament of Baptism. A sacrament is "an outward sign, instituted by Christ to confer grace." The water of baptism, the first of the sacraments, and its accompanying ritual has the deepest significance in our relationship with God, our Father, through Jesus Christ. It is our initiation to "life in the Spirit" and enlists us as members of the Christian communion. Very few people in this world have convinced themselves, that life is not spirit. Most of us inherently know that spirit or soul, is "the life of the body." Radical Secularism generally works against spirituality and the existence of God. People of that distinction defend the negative hypothesis that there is no God, however, they are unable to provide any positive proof of initial causality by any other conclusive means. Therefore, they become almost completely self oriented, but not necessarily without common ethics or a consensus morality.
while a wind from God swept over the face of the waters.
Then God said "let there be light;" and there was light.
Water, as an ablution, is used in practically all faiths. For Christians, John the Baptizer was the "voice crying in the wilderness;" the one whom Isaiah prophesied to be chosen by God to prepare the way of the Messiah. John was spiritually "cleansing" by the ritual of immersion those who were willing to repent of their sins against the God of Israel and "make straight the path" for the expected Messiah. It was Jesus who gave baptism sacramental significance when he allowed himself to be baptized by John in the Jordan River, "To fulfill all righteousness." This event also marked the beginning of his public ministry. The water of baptism became the specific effluence of divine grace, as things were made right between God and man by the coming of "the Lamb of God." Salvation had come through the Jews. Grace, truth, and new life in the Spirit came with the arrival of the "Chosen One of God." Being "born again" of water and the Spirit would become a necessary step for a regeneration of God's favor, with the promise of eternal life through the Risen One. A new covenant would be made with the blood of the Lamb – between God and man in Christ Jesus. The "Kingdom of God" was opened to all humanity.
Other clear and distinct sources of the sanctifying grace of God were instituted by Christ with the sacraments, especially the Eucharist which is the "body and blood, soul and divinity" of Christ himself. The seven sacraments are: Baptism, Confirmation, The Eucharist, Penance, Anointing of the Sick, Holy Orders and Matrimony. Those that are received only once, are Baptism, Confirmation, Holy Orders and Matrimony. The others are a continuous source of sanctifying grace through the Holy Spirit in the Church for those who embrace them faithfully and receive them worthily.


Water Pepper features two swirling floral jewels dating from the 1950s set to one side of a comfortable headband. Each jewel comprises glittering emerald and clear rhinestones in a goldtone setting. These are embellished with new emerald green Swarovski crystals.
Water pepper can be worn on either side of the head, each giving a slightly different look. The jewelled cluster measures 6 cm at its widest point and is 12 cm long. The band is wrapped with blonde satin ribbon.


Japanese guidelines for the management of acute pancreatitis: Japanese Guidelines 2015.
Isaji S, Takada T, Mayumi T, Yoshida M, Wada K, Yokoe M, Itoi T, Gabata T. J Hepatobiliary Pancreat Sci. 2015 Jun;22(6):433-45. doi: 10.1002/jhbp.260. PubMed PMID: 25904407.
Bakker OJ, Issa Y, van Santvoort HC, Besselink MG, Schepers NJ, Bruno MJ,Boermeester MA, Gooszen HG. Nat Rev Gastroenterol Hepatol. 2014 Aug;11(8):462-9. doi: 10.1038/nrgastro.2014.39. Epub 2014 Mar 25. Review. PubMed PMID: 24662281.
HPB (Oxford). 2015 Oct 17. doi: 10.1111/hpb.12491. [Epub ahead of print] PubMed PMID: 26475650.
Sabo A, Goussous N, Sardana N, Patel S, Cunningham SC. JOP. 2015 Mar 20;16(2):125-35. doi: 10.6092/1590-8577/2947. PubMed PMID: 25791545.
Necrotizing pancreatitis: new definitions and a new era in surgical management.
Lancet. 2015 Sep 26;386(10000):1261-8. doi: 10.1016/S0140-6736(15)00274-3. PubMed PMID: 26460661.
Räty S, Pulkkinen J, Nordback I, Sand J, Victorzon M, Grönroos J, Helminen H, Kuusanmäki P, Nordström P, Paajanen H. Ann Surg. 2015 Nov;262(5):736-41. doi: 10.1097/SLA.0000000000001469.PubMed PMID: 26583660.
The Atlanta Classification, Revised Atlanta Classification, and Determinant-Based Classification of Acute Pancreatitis: Which Is Best at Stratifying Outcomes?
Kadiyala V, Suleiman SL, McNabb-Baltar J, Wu BU, Banks PA, Singh VK. Pancreas. 2015 Oct 15. [Epub ahead of print] PubMed PMID: 26474431.
Sureka B, Bansal K, Patidar Y, Arora A. Gastroenterol Rep (Oxf). 2015 Jul 29. pii: gov036. [Epub ahead of print] Review. PubMed PMID: 26224684.


text:
/content/kw/en/destinations/flights-to-london/from-bali https://www.qatarairways.com/en-kw/search-results
London Heathrow London Heathrow Overcast
From Bali
Book flights from Bali to London with Qatar Airways
Flying from Bali
The tropical paradise island of Bali has to be one of the most popular luxury destinations in the world, and thanks to regular flights from Bali with Qatar Airways passengers can now travel between this beautiful location and the rest of the world in style.
The island's main airport, Ngurah Rai International Airport, is located in southern Bali and is a fascinating juxtaposition of ultra-modern facilities surrounded by reminders of the island's ancient heritage.
As you would expect, the staff are incredibly warm and welcoming, and are on hand to offer you any assistance you need to make your journey a more pleasant and stress-free one.
The official taxi counter is located outside the arrivals hall, and taxis are relatively cheap to and from all of the island's major destinations.
A single, multi-storey car parking area is located next to the terminals, and has a 2,000 spaces available for both short and long-term stay. Specially reserved spaces for disabled passengers are located close to the exit that leads to the terminal itself.
Arriving at Ngurah Rai International Airport
Passengers flying from Bali with Qatar Airways will need to head to the main Terminal, where all international departures leave from.
International arrivals and departures are located in the newer L-shaped terminal section, where there are 10 international gates, one of which has been modified to take the latest Airbus 380 aircraft.
The departure area has 62 check in counters, and a large lounge area for the convenience and comfort of passengers.
As with any international air hub, Ngurah Rai International Airport has a good selection of facilities and amenities to make the start of your journey comfortable and relaxing.
There are plenty of retail outlets selling both local crafts and luxury, high-end goods including jewellery and leather accessories. A large duty free area is available to passengers who have cleared customs, while the terminal also offers a good selection of restaurants and cafés offering on-the-go local cuisine or more substantial meals.
Travel to London's historic capital in complete comfort, with flights from Bali to London Heathrow with Qatar Airways providing you with a luxury flying experience. Our delicious in-flight cuisine and spacious seating are the envy of other airlines, and you'll receive award-winning service from the moment you check in. Every need will be catered for by friendly and attentive crew, providing you with the very best passenger experience from start to finish.
London is one of the most visited cities in the world, and from culture to history and art to architecture it's a city that challenges and excites at every turn. It has unparalleled open green spaces such as Hyde Park, and its monuments such as Buckingham Palace and the Tower of London are positively iconic. Enjoy fine dining, shopping and some of the most amazing sights in the world when you visit with Qatar Airways.
Arriving in London
From Big Ben to the London Eye, Buckingham Palace to the Shard and Nelson's Column, London is packed with attractions for visitors to discover. Book a flight to London with Qatar Airways and you'll be able to wander around this eclectic city that welcomes millions of visitors from around the world every year.
Pageantry and pomp, festivals and events – London has it all. Even its transport is iconic, with London red buses and black cabs recognised all over the world. Fly to London with Qatar Airways and you'll also discover world-class dining, exclusive shopping, luxury hotels and wellness centres, as well as surprises in every single one of its 32 boroughs.
Westminster probably has more iconic monuments and attractions packed into a small area than almost any other city in the world. Here you'll find the Houses of Parliament, Big Ben, Downing Street (the home of British government), Whitehall, the Lions and Nelson's Column in Trafalgar Square, and a host of other things to see.
Head out of Westminster to the west and you'll find some of London's greatest museums such as the Natural History Museum, the Science Museum, the Victoria and Albert and the National Gallery.
Newer attractions include the London Eye – a huge Ferris wheel that gives you a spectacular view over London. For a spot of pomp, head down to Buckingham Palace and watch the Changing of the Guard, or find an oasis of peace and quiet in one of the many parks dotted throughout the capital.
Flights to London with Qatar Airways land at London Heathrow, the world's busiest air transport hub. Visa restrictions for entry into the country will depend on your country of origin, length of stay and whether your trip is for business or pleasure.
Before you fly to London please check the visa and passport requirements.
Essential facts about London Heathrow


The city of Pamplona is world famous for the historic Running of the Bulls festival, celebrating the life of San Fermin. This annual event believed to have started in the 14th Century draws thousands of visitors eager to try their luck at outrunning the bulls. Although the city is mostly renowned for this iconic event, there is much more to discover including the beautiful medieval city centre, and an array of ambient dining venues and trendy bars.
The Running of the Bulls is an eight-day event in July where thrill-seekers take to the streets dressed head-to-toe in white – with a token red bandana. A rocket signals that the bulls have been released and the next four minutes involve a sea of people being chased throughout the city's cobblestone streets by thundering bulls heading towards the bullring.
Every evening the celebrations continue on the streets, with firework displays, dancing, music and partying till the early hours. You can also join the festivities as a part of a guided tour that includes exploring the city, organised parties and authentic dining experiences.
Join a guided tour and wander along the stone-paved streets of the city centre, visiting culturally significant attractions including the Gothic Pamplona Cathedral with its stunning Neo-classical facade. The compact size of the inner-city makes exploring a breeze, with the scenic La Taconera Park and Pamplona City Hall all within easy walking distance of one another.
A must-see attraction in Pamplona is the pentagon-shaped Citadel - a superb example of a Renaissance fortification, which today is an expansive park that can explored on a leisurely walking tour. Plaza del Castillo, known simply as the city's 'living room' is the city's main public square which is a popular spot to shop, relax and dine in the many quaint cafes.


GREEN pupils are to create their own beauty spot - with a little help from their friends!
This Saturday, staff and pupils of St Peter's Primary School, Brotton, will work in partnership with Marshall Drive Playing Field Action Group to develop a 'breathing place' as part of BBC Tees Springwatch.
From 10am to 2pm, children and volunteers will be planting wildflowers, trees, plants and erecting bird and bat boxes.
Volunteers of all ages are invited to come along. Meet in the car park on Marshall Drive Playing Field at 10am.


The San Joaquin and its tributaries, the Stanislaus, Tuolumne, and Merced Rivers together comprising the "San Joaquin Four Rivers Index", represent an important input into the California State Water Project, operated by the California Department of Water Resources (CADWR). In 2013-2014, David Meko and Ramzi Touchan (University of Arizona Laboratory of Tree-Ring Research) developed a reconstruction of the San Joaquin Four Rivers Index (900-2012), for the CADWR. Meko and Touchan also developed reconstructions for the Stanislaus River inflow to New Melones Lake, Tuolumne River inflow to New Don Pedro Reservoir, Merced River inflow to Lake McClure, and San Joaquin River inflow to Millerton Lake.
Water-year-total flows for San Joaquin Four Rivers were reconstructed by locally weighted regression, or Loess from subsets of 61 chronologies screened for Sacramento/San Joaquin basin reconstructions. A Loess reconstruction was defined as an interpolation of estimated flow from a smoothed scatterplot of observed flow on a single summary tree-ring variable. The tree-ring predictor was an average standard chronologies that were filtered and scaled to accentuate their statistical signal for the target flow gage. A time-nested-modeling approach was used for reconstructions, using progressively longer but smaller subsets of chronologies going back in time to calibrate subsets of reconstrutions. The percentage of flow variance accounted for by the "median-accuracy" model ranges from 68% for the Sacramento River (Sacramento River above Bend Bridge) to 78% for the San Joaquin River. Because these reconstructions are done with time-nested models, accuracy varies over time depending on the quality of the available tree-ring chronologies.
Note: the calibration and validation statistics above were computed during the model development and reflect the relationship between the log-transformed observed flows and the tree-ring predictors. The scatterplot below in Figure 1 shows the relationship between the back-transformed observed flows and the reconstructed flows, which has a lower R2 than that reported in the table. Also, the Standard Error of the Estimate and Root Mean Square Error reported above are in log units, and the RMSE can't be used to compute the confidence intervals.
Figure 1. Scatter plot of observed and reconstructed San Joaquin River annual flow, 1901-2012.
Figure 2. Observed (black) and reconstructed (blue) annual San Joaquin River annual flow, 1901-2012. The observed mean is illustrated by the dashed line.
Figure 3. Reconstructed annual flow fSan Joaquin Four Rivers (900-2012) is shown in blue. Observed flow is shown in gray and the long-term reconstructed mean is shown by the dashed line.
Figure 4. The 10-year running mean (plotted on final year) of reconstructed San Joaquin Four Rivers flow, 900-2012. Reconstructed values are shown in blue and observed values are shown in gray. The long-term reconstructed mean is shown by the dashed line.


A Modern Mixture with a Classic Finish, High Shine and Medium Hold. Water soluble formula combs into the hair with ease and is ideal for shaping well groomed looks including slicked back, side parts, low pompadour's, fades, textured crew cuts and more.
Distribute a dollop of POMADE between fingers & palms and work into wet or dry hair.
Wet Look / Softer Hold: Work evenly into wet hair, comb through and shape into style.
More Grip / Medium Hold: Create shape and volume using a blow dryer. Work pomade evenly into dry hair and comb through,shaping into style.


text:
COVID-19 risks for kids are low, must be balanced against cost of being out of school, doctors say | #covid19 | #kids | #childern | #parenting | #parenting | #kids
Nerissa Crichlow of Toronto has a lot of unanswered questions about what school will look like for her twin daughters in September.
"First and foremost, are they going to be splitting up the classes? What is that going to look like? Are there going to be testing measures in place?"
She describes herself as "very concerned" about the risk of her seven-year-old daughters, Mila and Norah, contracting and bringing home the coronavirus if in-person classes resume in the fall.
"I really need a good understanding of what the protocols are going to be. I'm asthmatic, my daughter is asthmatic, my father is asthmatic, and my mother has lung issues," she said.
"For me, it's really important that the schools have some testing involved, because we are all susceptible to the virus, more so than others."
Crichlow has plenty of company among Canadian parents who have questions about the looming school year, but the latest research shows young children are at low risk of getting or spreading the coronavirus that causes COVID-19, and that missing school can have long-term costs for a child's well-being.
In a classroom in Thailand's Pathum Thani province on July 1, old ballot boxes are repurposed into partitions as the Thai government eased isolation measures and reopened schools nationwide. (Athit Perawongmetha/Reuters)
Dr. Nisha Thampi understands parents' reticence about the return to class. The medical director of infection prevention and control at Children's Hospital of Eastern Ontario in Ottawa is both a pediatric infectious disease physician and a mother.
She said she's been encouraged, though, by recent study results that give more insight into children's risk of contracting the illness and of spreading it to others.
"It is with more information around the risk of transmission and infection that we can inform the policies for school setting and other community settings," said Thampi.
A large study from South Korea, published by the Centers for Disease Control and Prevention in the U.S., found that children nine and under infected others in their households just 5.6 per cent of the time, while children 10 to 19 spread the virus at the same rate as adults, nearly 19 per cent of the time.
And research continues to show that illness is usually mild in children.
A recent meta-analysis of 550 COVID-19 cases among children under 18 in China, Italy and Spain found just nine children had a severe case. One, who died, had underlying conditions.
Parents must be 'partners in care' to prevent spread
"There's good data that shows in the majority of cases, a child with COVID-19 has a symptomatic adult in the home who is also COVID positive," said Thampi.
That means some of the power for controlling the spread of illness within schools hinges on parents acting as "partners in care," teaching their kids about good hand hygiene and making sound decisions about their own physical distancing practices, she said.
While it made good sense to shut down schools at the beginning of the pandemic when we were just learning about COVID-19, we now have an opportunity to learn from other parts of the world that have reopened schools with new safety protocols in place, she said.
"I support families who are concerned about schools not being a safe place to return to, because I would suggest that a pre-pandemic school environment did not have the strategies in place to minimize infection spread," she said.
One issue, she said, was that many parents faced work pressures that made it difficult to keep sick children at home.
Working from home isn't possible for all jobs, but the pandemic has shown it is an option for many working parents. That, combined with a new vigilance around respiratory symptoms, may help establish new standards for keeping sick kids home from school.
"I think we will be returning to a school setting so long as the right policies are in place — a school setting that is safer in terms of infection transmission risks and that offers opportunities for learning, socialization and, importantly, peer-to-peer learning and development," Thampi said.
Dr. Michael Silverman, chief of infectious diseases at London Health Sciences Centre in London, Ont., said not enough attention is being paid to research on the impacts of children being out of school for months on end. (Craig Chivers/CBC News)
That could mean measures such as spreading kids apart from one another in smaller groups, training children on hygiene practices in school and doing some learning outdoors when weather permits, she said.
Now that children have been without the structure of school for many months, it's become apparent that eliminating all risk of school-based transmission comes at a cost, said Thampi.
Getting kids back to class between waves
That's a point Dr. Michael Silverman, chief of infectious diseases at London Health Sciences Centre and St. Joseph's Hospital in London, Ont., wants to make clear.
"So many times I hear, 'Well, you can't be too careful,' without recognizing the risks of being home," he said.
The research that's not getting enough attention these days are the studies on the repercussions of students being out of class, he said.
"If they miss school, there's long-term impact on their cognitive development, on their social development and their overall ability to function in society."
Of course, all children will be at a similar disadvantage because of school closures, but the impacts will still be there, he said.
A study from UNICEF Canada found that the COVID-19 pandemic is having an unprecedented impact on the lives of children and youth, citing disrupted routines and loss of education and other resources. The organization is calling on governments to "deliver new crisis mitigation measures" because children "cannot wait months or years to return to school."
Given that children under 10 pose little risk of infection transmission to others, it makes sense to return their cohort to class, said Silverman.
Teacher Janick Mille welcomes students at Ecole Marie Rose in Saint Sauveur, Que., as elementary schools outside the greater Montreal reopened back on May 11. (Ryan Remiorz/The Canadian Press)
"If they're the least likely to get sick, they're the least likely to transmit, and they do worse with distance learning, the priority should be at least the very young children should be able to get back to school," he said.
As September approaches, teacher unions are asking for clear plans for safely reopening schools. The Ontario English Catholic Teachers Association, for example, has called on the provincial government to give direction to school boards about their responsibilities to ensure the safety of students and staff.
Silverman points out that most infectious disease experts anticipate a second wave of the illness will come.
"If we don't take advantage of the time when we're at a relatively low level of transmission, when another high level of transmission comes … and then we close the schools again, there will be an extremely long period of time with no education."
Silverman said he believes the choice should remain with parents as to whether their kids learn in the classroom — with best practices for infection-control in place — or from home.
"What I'm advocating is that we should not close all schools and take away all parents' choice. That parents should be able to make educated choices on behalf of their children as to what they feel is best for their family."