text:
Васи́лий Васи́льевич Спивако́в (3 апреля 1942, Ухта) — советский боксёр и тренер по боксу. На соревнованиях представлял спортивное общество «Трудовые резервы», мастер спорта СССР. Известен как тренер спортивного клуба «Олимпийские надежды» и СДЮШОР № 4 в Воронеже, личный тренер титулованного воронежского боксёра Владимира Ерещенко, заслуженный тренер РСФСР (1989).

Биография
Василий Спиваков родился 3 апреля 1942 года в городе Ухта Коми АССР, впоследствии переехал на постоянное жительство в Воронеж.

В молодости сам серьёзно занимался боксом, проходил подготовку на отделении бокса воронежской Детской спортивной школы № 6 под руководством тренера Александра Ивановича Чернова. В 1962 году одержал победу на первенстве центрального совета всесоюзного добровольного спортивного общества «Трудовые резервы» и выполнил тем самым норматив мастера спорта СССР.

После завершения спортивной карьеры перешёл на тренерскую работу, в течение многих лет работал тренером по боксу в воронежском спортивном клубе «Олимпийские надежды», занимал должность директора воронежской Специализированной детско-юношеской школы олимпийского резерва № 4.

За долгие годы тренерской деятельности подготовил многих талантливых спортсменов. Один из самых известных его учеников — мастер спорта международного класса Владимир Ерещенко, бронзовый призёр чемпионата мира и Игр доброй воли, серебряный призёр чемпионата Европы, участник летних Олимпийских игр в Сеуле. За подготовку этого спортсмена в 1989 году Василий Спиваков был удостоен почётного звания «Заслуженный тренер РСФСР». Другой его воспитанник — мастер спорта международного класса Олег Колядин, чемпион СССР среди юниоров, бронзовый призёр взрослого всесоюзного первенства, победитель международных турниров на Кубе и в Румынии, участник Кубка мира 1981 года. Также в разное время его подопечными были такие воронежские боксёры как Игорь Иванов, Анатолий Косматых, Юрий Фалеев, Андрей Князев и др.

Примечания

Ссылки
 Спиваков Василий Васильевич — страница на сайте «Спорт-страна.ру»

Боксёры СССР
Мастера спорта СССР
Тренеры по боксу СССР
Тренеры России по боксу
Заслуженные тренеры РСФСР


When Phyllis Arnold toured Old Québec with her husband a few years ago, a class of grade-seven students on a field trip caught her eye: the textbook they were using to learn about Quebec and Canada happened to be one of her own. Although she retired eight years ago, Arnold, a Governor and Fellow of The Royal Canadian Geographical Society, still runs into some of the 76 educational books she authored during her career. Arnold Publishing Ltd, the company she started with $50 in 1967, became one of the most successful independently owned educational book publishers in Canada.
"It's a real challenge to take complex historical and geographical concepts and make them into something that children learn from," explains Arnold. She designed her books for "the visual learner of today," using pictures and simulation games such as Marooned — in which a class is stranded on an imaginary island — to help students remember facts.
Leane de Laigue, a high school environmental studies teacher in Vancouver, will remember Arnold for more than her books. Last year, the Canadian Council for Geographic Education presented her with the Phyllis Arnold Professional Development Award, established by Arnold in 2001 to help educators attend professional-development courses and workshops. De Laigue used the subsidy to take courses in navigational skills and wilderness survival. "I just wanted to be more comfortable when I take students into the wilderness," she says. Arnold, a former schoolteacher in Edmonton, says it's important for teachers to branch out beyond the classroom and "get a feel" for what is going on in geographic education.


Animus Heart, a smart home controller in Google Home.
Animus Heart along with Google Assistant brings voice control to all your smart home devices like switches, lights and others – even if they're Z-Wave devices. Speak to your voice control system in any language and let Animus Heart do the rest. Although, the only way to make this possible is for you to tell your Assistant that Animus Heart is your smart home controller.
Allow your Heart to communicate with Google Assistant.
English, being a predominant language worldwide, could be a restriction if it's not your primary language. It would be helpful to be able to use commands in your own language once in a while, and so, controlling your smart devices with Animus Heart could make this easier as it allows multiple languages to work with the Animus-Google integration. It expands the dimensions of your voice controlled smart home and makes the experience better by supporting the voice control feature in your own language.
Speak simple, more direct sentences.
Giving one command at a time can make the Heart and Assistant communicate better with each other.
For Your Information: Google Assistant is currently available in English, Danish, Dutch, French, German, Hindi, Italian, Indonesian, Japanese, Korean, Norwegian, Polish, Portuguese (Brazil), Russian, Spanish, Swedish, Thai, and Turkish. Keep checking for more languages that might be added.


ROSALIND I. DELA CRUZ, R.N.
Proper care of wounds can prevent infection and speed up the body's healing process.
Immediately after the injury, wash thoroughly with clean water and mild soap. Remove any visible dirt or debris from the wound. Apply gentle pressure to stop bleeding.
For burn wounds, run cool water over the area or apply a cool, wet cloth. If blisters form, do not pop or drain.
Apply a thin layer of bacitracin antibiotic ointment or white petroleum to the wound. Cover with a bandage.
Clean area twice daily with soap and water, and apply a new bandage and ointment after cleaning. There is no need to use hydrogen peroxide or alcohol for cleaning. Continue this care until wound is fully healed.
Tetanus is an uncommon but serious infection that can occur after a skin injury. It is recommended that all individuals receive a series of three tetanus vaccinations, usually given during infancy, and a booster shot every 10 years. Some puncture wounds or other dirty wounds may require a tetanus booster if it has been more than five years since the last tetanus shot.
• Any concerns about poor healing, large or gaping wounds, bite injuries, etc.


text:
\section{\label{sec:level1} Introduction}
\section{Introduction \label{sec:level1}}

Gravitational wave (GW) astronomy was unveiled by the first detection of advanced LIGO and Virgo -- GW150914 \cite{Abbott:2016blz}. Tens of detections have been confirmed during the advanced LIGO and Virgo O1 and O2 runs including the additional new candidates \cite[and references therein]{TheLIGOScientific:2016pea,LIGOScientific:2018mvr,Venumadhav:2019lyq,Nitz:2019hdf}. The GW detection, GW170817, and electromagnetic counterparts observations from binary neutron stars merger opened a new multi-messenger era \cite[and references therein]{TheLIGOScientific:2017qsa,GBM:2017lvd}. Scores of candidates have been preliminarily identified by advanced LIGO and Virgo with upgraded sensitivity during the O3 run from April 2019 to March 2020 \cite{gracedb}, and a new binary neutron stars detection, GW190425, has been confirmed \cite{Abbott:2020uma}. KAGRA started its observation from February 25th, 2020 \cite{KAGRA}, and ground-based network  would enter the four interferometers era.

The space missions targeting for low-frequency GW detections are expected to be launched in the 2030s. With LISA Pathfinder successfully demonstrated the drag-free technology and GRACE follow-on testing the laser metrology, the essential technologies for LISA mission are reaching maturity and paving the path for its launch in the 2030s \cite{2017arXiv170200786A,Armano:2016bkm,Armano:2018kix,Abich:2019cci}. In China, two space missions are proposed to detect the GW in low frequency band -- TAIJI \cite{Hu:2017mde} and TianQin \cite{Luo:2015ght}. The TAIJI mission is considered to use a LISA-like formation in a heliocentric orbit, and TianQin is considered to be in a geocentric orbit. TAIJI and TianQin launched their respective pathfinders, TAIJI-1 in August \cite{Luo:2020} and TianQin-1 in December \cite{Tianqin-1} of 2019, testing the first stage of development of their accelerometers, metrology, and others technologies in space.

As the L3 mission of ESA's Cosmic Vision 2015–25 plan, LISA is considered to be promoted to an earlier launch time alongside the L2 mission -- Athena \cite{ESAnews}. Athena is a space mission with new generation spatially-resolved X-ray spectroscopy and deep wide-field X-ray spectral imaging system, and targeting to observe the energetic processes in the universe \cite{2013arXiv1306.2307N}. The joint observations from LISA and Athena can boost the understanding of the basic physics and astrophysics of the universe \cite{Colpi:2019}. One apparent scenario could be that LISA detects the GWs from sources and identify their sky locations for Athena's follow-up observations \cite{2020NatAs.tmp....4M}.

The angular resolutions of LISA for binary black holes and monochromatic sources have been studied since the original LISA proposed \cite{Cutler:1997ta,1997CQGra..14.1507P,1998AIPC..456...95C}, with more detailed studies thereafter \cite[and references therein]{Vecchio:2004ec,2007PhRvD..76j4016A,2008arXiv0806.1591B,2016PhRvL.116w1102S}. The investigations usually adopted the averaged sensitivity and treated LISA as two independent interferometers. This approach should be enough to estimate the average performance.
\citet{Vallisneri:2012np} pointed out that SNR from an average sensitivity is not accurate for individual sources, and parameter estimation could be imprecise due to response to a GW signal vary with frequency and orientation. On the other hand, time-delay interferometry (TDI) is required for LISA-like missions to suppress the laser frequency noise. The response of a TDI combination to a GW signal is formed by combining the measurements from time shifted laser links. \citet{2010PhRvD..81f4014M,2011PhRvD..84f4003M} investigated the TDI responses, especially in the optimal-A, E and T channels, for GW detections and parameter estimations.

To simulate the TDI effects in the LISA measurements, multiple simulators were developed.
The Synthetic LISA is developed to simulate the LISA science process at the level of scientific and technical requirements \cite{Vallisneri:2004bn}.
LISACode is developed to bridge the gap between the basic principles of LISA and sophisticated simulator \cite{2008PhRvD..77b3002P}, and its successor LISANode is newly developed to adapt to the updated LISA measurements \cite{2019PhRvD..99h4023B}.

Besides the angular resolution investigations for solo LISA mission, \citet{Crowder:2005nr,2016PhRvD..94h1101T,Tinto:2017kre} also explored the sky localization improvement with LISA and other presumed detector(s).
TAIJI is expected to be launched in the 2030s and could have observation period overlapped with LISA and Athena. It is considered to be a heliocentric orbit mission in front of Earth by around 20$^\circ$. With large distance separation, LISA and TAIJI could form a network and bring abundant merits for the GW observations.
By using the average sensitivity, \citet{Ruan:2019tje} estimated that the joint observation of LISA and TAIJI could significantly improve the sky localization precision for the supermassive black hole (SMBH) binaries.

In this work, by using the numerical orbit achieved and a simulator developed, we numerically calculate the sky- and polarization- averaged sensitivities for various TDI channels of LISA and TAIJI based on the updated missions' requirements. Then we investigate the sky localization merits from LISA and TAIJI joint observation for the coalescing SMBH binaries and monochromatic sources considering the response of specific TDI configurations.
We organize our paper as follows. In Section \ref{sec:orbit}, we introduce the numerical orbits we achieved for LISA and TAIJI missions. In Section \ref{sec:TDI}, we describe the noise assumptions, TDI response to GW signals in TDI channels and their corresponding sensitivities. In Section \ref{sec:SMBH}, we report the simulation on the sky localization performance of LISA-TAIJI joint observation for coalescing SMBH binaries. In Section \ref{sec:mono}, we present the simulation of sky localization for the monochromatic sources by using the LISA and TAIJI network. And we recapitulate our conclusions and discussions in Section \ref{sec:conclusions}.

\section{Numerical Mission Orbit} \label{sec:orbit}

LISA mission originally proposed an equilateral triangle constellation with $5 \times 10^6$ km laser links to detect the low-frequency GWs \cite{LISA2000}. The formation has a $60^\circ$ inclination angle with respect to the ecliptic plane and trails the Earth by about $20^\circ$. After NASA's withdrawal from ESA-NASA LISA collaboration in 2011, the LISA mission evolved to a down-scaled mission, so called eLISA/NGO, which was supported by the European countries (France, Germany, Italy, the Netherlands, Spain, Switzerland and the UK) and ESA. In 2017, LISA team proposed a new LISA configuration with $2.5 \times 10^6$ km arm length and $20^\circ$ trailing angle \cite{2017arXiv170200786A}. The schematic is shown in Fig. \ref{fig:orbit-scheme}.

TAIJI program is a LISA-like mission proposed by Chinese Academy of Sciences \cite{Hu:2017mde,Luo:2020}. Three spacecraft (S/C) form a triangle constellation with $3 \times 10^6$ km arm length. The constellation could be leading or trailing the Earth by $20^\circ$ on the heliocentric orbit. Considering the merits of LISA-TAIJI joint observation with large separation, the current mission trend is to be localized in front of Earth as shown in Fig. \ref{fig:orbit-scheme} \citet{Ruan:2019tje}.
\begin{figure}[htb]
\includegraphics[width=0.45\textwidth]{./LISA_TAIJI_orbit.eps}
\caption{\label{fig:orbit-scheme} The schematic of LISA and TAIJI orbit.}
\end{figure}

The studies of LISA(-like) orbit have been going on for more than two decades. \citet{Folkner:1997hn} estimated the LISA orbit stability by using an analytical method. \citet{Dhurandhar:2004rv} and \citet{Nayak:2006zm} formulated and optimized the LISA(-like) orbit formation analytically by using Clohessy-Wiltshire frame. \citet{Wu:2019thj} expanded the orbital equations in \citet{Dhurandhar:2004rv} to the higher order of the eccentricity and applied to the TAIJI mission orbit. In two companion papers, \citet{Yi:2008zza} employed coorbital restricted problem to design the LISA orbit and \citet{Li:2008al} introduced an algorithm to optimize the orbit numerically.

In our previous works \cite{Wang:2011,Wang:2014aea,Wang:2012ce,Wang:2012te,Dhurandhar:2011ik,Wang:2014cla,Wang:2017aqq,Wang:2019ipi}, we developed a workflow to design and optimize the drag-free orbit of a GW space mission by using an ephemeris framework, and calculate the time difference of the TDI paths. In our recent work \citep{Wang:2017aqq}, we worked out a LISA mission orbit based on the new requirements in its proposal \citep{2017arXiv170200786A}. Furthermore, we applied the procedures to TAIJI mission and achieved an optimized orbit at the same trailing angle and epoch \cite{Wang:2017aqq}. In this work, along the workflow we developed, we obtain an optimized orbit for TAIJI mission in front of the Earth by $20^\circ$ to study the merits of the LISA-TAIJI joint observation.

We refer the specific formulation and optimization method for LISA-like orbits to our previous works \cite{Wang:2012ce,Dhurandhar:2011ik,Wang:2017aqq}. In this section, we briefly summarize our procedures of workflow as follow: 1) determine the starting time of a mission; 2) obtain the initial condition by using the formula (e.g. Equation (2.1)-(2.6) in \cite{Wang:2012ce}); 3) put the initial conditions of the celestial bodies and S/C to the ephemeris framework and calculate the orbit by using numerical integration; 4) adjust the orbital periods and eccentricities of the S/C iteratively to meet the mission requirements; and 5) expand the achieved orbit to the backward time direction and truncate the time period which satisfied the requirements that can prolong the effective mission time.

To calculate the orbit accurately, the interactions considered in our ephemeris framework CGC3.0 include, 1) the Newtonian and first-order post-Newtonian interaction between Sun, major planets, Pluto, Moon, Ceres, Pallas and Vesta; 2) the figure interactions between Sun/Earth/Moon and others as point mass bodies; 3) the perturbations from selected 340 asteroids and 4) the tide effects on Moon from the Earth. For a starting time, the CGC3.0 firstly read constants, positions and velocities of the celestial bodies from DE430, and then integrate the orbits of the celestial bodies/spacecraft by using the equations of motion considered. The heliocentric distance of Earth calculated by CGC3.0 is less than 0.3 m in 10 years comparing to the ephemeris DE430 \cite{DE430}.

Based on the orbital requirements for new LISA \cite{2017arXiv170200786A}, we set the optimization criteria: 1) the relative velocities between S/C should be smaller than 5 m/s; and 2) the effective mission duration should be longer than 4 years. For TAIJI mission, due to the larger arm length, we set the criteria of the relative velocities to be less than 6 m/s. The optimized orbits achieved for LISA and TAIJI missions are shown in Fig. \ref{fig:orbit}. These numerical orbits start on March 22nd, 2028 (JD2461853.0) and can maintain in required status for 2200 days ($\sim$6 years). The relevant equations for the ephemeris calculation and for choosing the initial conditions of S/C are assembled in Appendix A.
\begin{figure*}[htb]
\includegraphics[width=0.48\textwidth]{./LISA_ArmLength.eps}
\includegraphics[width=0.48\textwidth]{./TAIJI_ArmLength.eps} \\
\includegraphics[width=0.48\textwidth]{./LISA_RelVel.eps}
\includegraphics[width=0.48\textwidth]{./TAIJI_RelVel.eps}
\caption{\label{fig:orbit} The numerical LISA and TAIJI orbit achieved and used in the hereafter simulation. The arm length variations with mission time are shown in the upper row (upper left for LISA and right for TAIJI). The relative velocities between S/Cs are shown in the lower row (lower left for LISA and lower right for TAIJI).}
\end{figure*}

It is needed to emphasize that the orbit shown in Fig. \ref{fig:orbit} are the geodesics of three S/C in the solar system barycentric (SSB) coordinate system without considering an orbital maneuver. \citet{Bender:2013mma} proposed the periodic maneuver control for eLISA mission orbit and evaluated the requirement for the thruster. \citet{Halloin:2017tzi} presented an optimization method for the numerical orbit including the periodic orbital maneuvers. A group of orbital maneuvers could be implemented to our achieved orbit to extend the mission duration. In our recent work, we also explored the possibility that to maintain a constant arm triangular constellation by using thruster propulsion \cite{Wang:2019ipi}.

\section{Time-Delay Interferometry} \label{sec:TDI}

For a LISA-like space mission, TDI is essential to achieve the sensitivity goal. The principle of TDI is to properly time shift and combine the data streams to suppress the laser frequency noise and preserve the GW signals. Two generations of TDI combinations were proposed and studied for LISA mission depending on their demands to cancel the laser frequency noise \cite[and references therein]{1999ApJ...527..814A,2000PhRvD..62d2002E,2001CQGra..18.4059A,Prince:2002hp,Dhurandhar:2002zcl,Cornish:2003tz,2003PhRvD..67l2003T,Vallisneri:2005ji,Tinto:2014lxa,Vallisneri:2007xa,Vallisneri:2012np}. The first-generation TDI combination can cancel the frequency noise in a stationary unequal-arm interferometry, and the second-generation TDI combinations are targeting to further cancel the frequency noise in a moving interferometer. In this work, we focus on the investigation of the first-generation TDI combinations.

The first-generation TDI combinations are classified as five configurations which are Sagnac $(\alpha, \beta, \gamma)$, unequal-arm Michelson (X, Y, Z), Relay (U, V, W), Beacon (P, Q, R) and Monitor (E, F, G), plus symmetric Sagnac $\zeta$. To distinguish from the optimal TDI channel E hereinafter, we use the (D, F, G) to indicate the Monitor channels instead. The three channels in each configuration are obtained by cyclical permutation of the spacecraft indexes. Except for the Sagnac, the first channel for each configuration are shown in Fig. \ref{fig:TDI1st_path}.
\begin{figure*}[htb]
\includegraphics[width=0.22\textwidth]{./MichelsonX.eps}
\includegraphics[width=0.2\textwidth]{./RelayU.eps}
\includegraphics[width=0.22\textwidth]{./BeaconP.eps}
\includegraphics[width=0.2\textwidth]{./MonitorD.eps}
\caption{\label{fig:TDI1st_path} The diagram of selected channels (Michelson-X, Relay-U, Beacon-P and Monitor-D) from first-generation TDI configurations \cite{Vallisneri:2005ji}. }
\end{figure*}

\subsection{Noise PSDs of TDI channels} \label{secsub:TDI_noise}

Under the assumption that laser frequency noise has been canceled by TDI combinations, only acceleration noise and optical path noise are considered in our simulation. The current requirements of acceleration noise $S_{\rm acc}$ for LISA and TAIJI are the same which are \cite{2017arXiv170200786A,Luo:2020},
\begin{equation}
 S^{1/2}_{\rm acc} \leq 3 \times 10^{-15} \frac{\rm m/s^2}{\sqrt{\rm Hz}} \sqrt{1 + \left(\frac{0.4 {\rm mHz}}{f} \right)^2 }  \sqrt{1 + \left(\frac{f}{8 {\rm mHz}} \right)^4 }.
\end{equation}
The requirement of optical path noise $S_{\rm op}$ for LISA and TAIJI mission are slightly different:
\begin{equation}
\begin{aligned}
 S^{1/2}_{\rm op, LISA} &\leq 10 \times 10^{-12} \frac{\rm m}{\sqrt{\rm Hz}} \sqrt{1 + \left(\frac{2 {\rm mHz}}{f} \right)^4 },  \\
S^{1/2}_{\rm op, TAIJI} &\leq 8 \times 10^{-12} \frac{\rm m}{\sqrt{\rm Hz}} \sqrt{1 + \left(\frac{2 {\rm mHz}}{f} \right)^4 }.
 \end{aligned}
\end{equation}
By assuming there is no correlation between the different test masses and optical benches, the power spectral density (PSD) functions of selected first-generation TDI configurations/channels are \cite{1999ApJ...527..814A,2000PhRvD..62d2002E,2001CQGra..18.4059A,Vallisneri:2007xa,Vallisneri:2012np}
\begin{equation} \label{eq:Sn_XUD}
\begin{aligned}
S_{\rm X} (f) = & 16 S_{\rm op} (f) \sin^2 x \\ &+ 16 S_{\rm acc} (f) (3 + \cos 2x ) \sin^2 x , \\
S_{\rm U} (f)  = & 8  S_{\rm op}  (4 + 4  \cos x +  \cos 2x )  \sin^2 (x/2) \\ &+ 16  S_{\rm acc}  (5 + 5   \cos x + 2   \cos 2x )  \sin^2 (x/2) , \\
S_{\rm D} (f) = & S_{\rm P} (f) =  8  S_{\rm op}  (3 + 2  \cos x)  \sin^2 (x/2) \\ &+ 16  S_{\rm acc}  (3 +  \cos x )  \sin^2 (x/2) ,
\end{aligned}
\end{equation}
where $x = 2 \pi f L$. The PSD curves of these four TDI channels for LISA and TAIJI are shown in Fig. \ref{fig:TDI1st_noise} upper panel.

A group of optimal TDI channels could be obtained by linear combinations of the three channels in one TDI configuration, (e.g. Sagnac TDI configuration used in \citet{Prince:2002hp}). In our investigation, we apply the Michelson TDI configuration, (X, Y, Z), to compose the optimal TDI configurations as used in \citet{Vallisneri:2007xa},
\begin{equation} \label{eq:optimalTDI}
 {\rm A} =  \frac{ {\rm Z} - {\rm X} }{\sqrt{2}} , \quad {\rm E} = \frac{ {\rm X} - 2 {\rm Y} + {\rm Z} }{\sqrt{6}} , \quad {\rm T} = \frac{ {\rm X} + {\rm Y} + {\rm Z} }{\sqrt{3}}.
\end{equation}
The corresponding PSD functions of noise for these three channels are
\begin{equation} \label{eq:Sn_AET}
\begin{aligned}
 S_{\rm A} =  S_{\rm E} = & 8  S_{\rm op}  (2+\cos x ) \sin^2 x \\ & + 16  S_{\rm acc}  (3+ 2 \cos x + \cos 2x )  \sin^2 x, \\
 S_{\rm T} = & 16  S_{\rm op} (1 - \cos x ) \sin^2 x \\ & + 128  S_{\rm acc} \sin^2 x \sin^4(x/2).
\end{aligned}
\end{equation}
The PSD curves for LISA and TAIJI are shown in Fig. \ref{fig:TDI1st_noise} lower panel. It's needed to emphasize that the PSD function in Eq. \eqref{eq:Sn_XUD} and \eqref{eq:Sn_AET} are achieved by assuming the fully equal arm configuration. For an unequal arm configuration, the PSD of T channel could be divergent from expected at lower frequency band  as shown by the curves of mission-T and mission-T-EqualArm.
\begin{figure}[htb]
\includegraphics[width=0.48\textwidth]{./LISA_TAIJI_TDI1st_noise.eps} \\
\includegraphics[width=0.48\textwidth]{./LISA_TAIJI_XAET_noise_UnequalArm.eps}
\caption{\label{fig:TDI1st_noise}The PSD of selected first-generation TDI channels (Michelson-X, Relay-U, Beacon-P, and Monitor-D) for LISA and TAIJI (upper panel), the PSD of the optimal TDI channels (A, E and T) and X channel (lower panel). The mission-T curves show the PSD of T channel at the starting time of the numerical orbits, and the mission-T-EqualArm curves show the PSD of T channel by using the Eq. \eqref{eq:Sn_AET} which is for fully equal arm configuration. (The curves of P and D channels are fully overlapped in the upper panel, as well as the A and E channel in the lower panel.) }
\end{figure}

\subsection{Response of TDI to GW} \label{secsub:TDI_response}

\citet{1975GReGr...6..439E} formulated the response to a GW signal in a single link Doppler measurement. A TDI channel is connected by multiple laser links, the final response to a GW signal is combined by each single link. Furthermore, the response of each TDI configuration to a same GW source could vary with relative position, orientation and frequency. Referring to the formulas in \citet{Vallisneri:2012np}, we briefly state the response functions applied in our simulation. Different from using their analytical orbit, we adopt the numerical orbit achieved in Section \ref{sec:orbit}.

For a GW source locate at direction $(\lambda, \beta)$, where $\lambda $ and $\beta$ is the ecliptic longitude and latitude in the SSB coordinates, the propagation vector is described as
\begin{equation}
 \hat{k}  = -( \cos \lambda \cos \beta, \sin \lambda \cos \beta ,  \sin \beta ).
\end{equation}
The polarization tensors of plus and cross of GW signal are
\begin{equation}
\begin{aligned}
{\rm e}_{+} & \equiv \mathcal{O}_1 \cdot
\begin{pmatrix}
1 & 0 & 0\\
0 & -1 & 0 \\
0 & 0 & 0
\end{pmatrix}
\cdot \mathcal{O}^T_1 ,
\ \
{\rm e}_{\times} & \equiv \mathcal{O}_1 \cdot
\begin{pmatrix}
0 & 1 & 0\\
1 & 0 & 0 \\
0 & 0 & 0
\end{pmatrix}
\cdot \mathcal{O}^T_1,
\end{aligned}
\end{equation}
with
\begin{widetext}
\begin{equation}
\mathcal{O}_1 =
\begin{pmatrix}
\sin \lambda \cos \psi - \cos \lambda \sin \beta \sin \psi & -\sin \lambda \sin \psi - \cos \lambda \sin \beta \cos \psi & -\cos \lambda \cos \beta  \\
     -\cos \lambda \cos \psi - \sin \lambda \sin \beta \sin \psi & \cos \lambda \sin \psi - \sin \lambda \sin \beta \cos \psi & -\sin \lambda \cos \beta  \\
         \cos \beta \sin \psi & \cos \beta \cos \psi & -\sin \beta
\end{pmatrix},
\end{equation}
where $\psi$ is the polarization angle.

The response in a single link measurement from S/C$i$ to $j$ is described by \cite{Vallisneri:2007xa}
\begin{equation}
\begin{aligned}
y^{\rm{GW}}_{ij} (f) =&  \frac{ (1 + \cos^2 \iota ) \hat{n}_{ij} \cdot {\rm e}_+ \cdot \hat{n}_{ij} + i (- 2 \cos \iota ) \hat{n}_{ij} \cdot {\rm e}_\times \cdot \hat{n}_{ij} }{4 (1 - \hat{n}_{ij} \cdot \hat{k} ) }
 \times \left[  \exp( 2 \pi i f (L_{ij} + \hat{k} \cdot p_i ) ) -  \exp( 2 \pi i f  \hat{k} \cdot p_j )  \right] ,
\end{aligned}
\end{equation}
\end{widetext}
where $\hat{n}_{ij}$ is the unit vector from SC$i$ to $j$, $L_{ij}$ is the arm length along the SC$i$ and $j$, $p_i$ is the position of the S/C$i$ in the SSB coordinates. and $\iota$ is the inclination of the GW source from the line of sight.

For the four first-generation TDI channels (Michelson-X, Relay-U, Beacon-P and Monitor-D), the response expressions in frequency-domain could be described by linear combination of each link measurement with/without time delay factor(s),
\begin{widetext}
\begin{equation}
\begin{aligned}
 F^{\rm{GW}}_{ \rm X} (f) =& (-\Delta_{21} + \Delta_{21}  \Delta_{13}  \Delta_{31})  y^{\rm GW}_{12}
         + (-1 + \Delta_{13}  \Delta_{31} )  y^{\rm GW}_{21}
         + (\Delta_{31} - \Delta_{31}  \Delta_{12}  \Delta_{21})  y^{\rm GW}_{13}
         + ( 1 - \Delta_{12}  \Delta_{21} )  y^{\rm GW}_{31}, \\
F^{\rm{GW}}_{ \rm U} (f) =& (1 - \Delta_{32}  \Delta_{21}  \Delta_{13})  y^{\rm GW}_{23}
         + (\Delta_{23} - \Delta_{21}  \Delta_{13})  y^{\rm GW}_{32}
         + (\Delta_{32}  \Delta_{23} - 1)  y^{\rm GW}_{13}
         + (\Delta_{13} \Delta_{23}  \Delta_{32} - \Delta_{13})  y^{\rm GW}_{21}, \\
F^{\rm{GW}}_{ \rm P} (f) =& (\Delta_{13} - \Delta_{12}  \Delta_{23})  y^{\rm GW}_{32}
         + (\Delta_{13}  \Delta_{32} - \Delta_{12})  y^{\rm GW}_{23}
         + (\Delta_{13}  \Delta_{32}  \Delta_{23} - \Delta_{13})  y^{\rm GW}_{12}
         + (\Delta_{12} - \Delta_{12}  \Delta_{23}  \Delta_{32})  y^{\rm GW}_{13}, \\
F^{\rm{GW}}_{ \rm D} (f) =& (1 - \Delta_{23}  \Delta_{32})  y^{\rm GW}_{21}
         + (\Delta_{21} - \Delta_{31}  \Delta_{23})  y^{\rm GW}_{32}
         + (\Delta_{21}  \Delta_{32} - \Delta_{31})  y^{\rm GW}_{23}
         + (\Delta_{23}  \Delta_{32} - 1)  y^{\rm GW}_{31} ,
\end{aligned}
\end{equation}
\end{widetext}
where $\Delta_{ij} = \exp(2 \pi i f L_{ij})$.
To evaluate the detectability of a TDI channel, its response could be averaged over sky and polarization at a given frequency by
\begin{equation} \label{eq:resp_averaged}
\begin{aligned}
 \mathcal{R}^2_{\rm TDI} (f) =& \frac{1}{4 \pi^2}  \int^{2 \pi}_{0} \int^{\frac{\pi}{2}}_{-\frac{\pi}{2}} \int^{\pi}_{0} |F^{\rm{GW}}_{ \rm TDI} (f, \iota=0)|^2 \cos \beta {\rm d} \psi {\rm d} \beta {\rm d} \lambda.
\end{aligned}
\end{equation}
The averaged responses of four TDI channels (Michelson-X, Relay-U, Beacon-P, and Monitor-D) at different frequencies are shown in Fig. \ref{fig:response_1st} upper panel. As we can read from the plot, the unequal-arm Michelson-X combination has the best response in these four cases, and the curves of Beacon-P and Monitor-D channels are identical.
The lower panel of Fig. \ref{fig:response_1st} shows the optimal channels (A, E, T) comparing to the Michelson-X. The responses of optimal-A and E are identical and slightly higher than the Michelson-X channel. Although the averaged responses for optimal-A and E are the same, the instant sensitive directions of them could be different.
In the lower frequency band, the response of optimal-T channel is several orders lower than other TDI channels. On the other hand, considering the arm lengths vary with time, the average response of a TDI channel also can fluctuate. The curves shown in Fig. \ref{fig:response_1st} are calculated at the starting time of the mission orbits. For comparison, the response of T channel for fully equal arm configuration is shown by the curves LISA-T-EqualArm and TAIJI-T-EqualArm in Fig. \ref{fig:response_1st} lower panel.
\begin{figure}[htb]
\includegraphics[width=0.48\textwidth]{./LISA_TAIJI_resp_XUPD.eps}
\includegraphics[width=0.48\textwidth]{./LISA_TAIJI_resp_XAET_EqualArm.eps}
\caption{\label{fig:response_1st} The average responses of selected TDI channels at different frequencies. The regular TDI channels (Michelson-X, Relay-U, Beacon-P and Monitor-D) are plotted in the upper panel, and optimal-A, E and T channels with Michelson-X are shown in the lower panel. (The curves of P and D channels are fully overlapped in the upper panel, as well as the A and E channel in the lower panel). For comparison, the response of T channel for fully equal arm configuration are shown by curves LISA-T-EqualArm and TAIJI-T-EqualArm.}
\end{figure}

\subsection{Sensitivities of TDI channels}

Based on the noise assumptions and average response, the PSD of average sensitivity in one TDI channel could be obtained by weighting the PSD of noise by the averaged response, $S_{\rm avg} = {S_{\rm n}}/{\mathcal{R}^2}$.
The sensitivities of LISA and TAIJI on various TDI channels at the starting time are shown in Fig. \ref{fig:Sensitivity_1st}. Because of lower optical path noise requirement and longer arm length, TAIJI achieves slightly better sensitivities than LISA. For sensitivities from different TDI channels, the main divergences appear at the most sensitivity band, $\sim$[2, 50] mHz as shown in the amplified figures. The optimal-T channel has obvious divergence from others in the frequency band $\sim$[0.5, 50] mHz, and tends to have the same sensitivity as other channels when the frequency is lower than 0.5 mHz. This is different from the T channel results in \cite{Prince:2002hp,Vallisneri:2007xa} which assuming the equal arm.

Our further investigations show that the response of T channel to GW is proportional to the square of arm length differences at low frequency ($2 \pi f L \ll 1$) \cite{Wang:2020ongoing},
\begin{equation}
 \mathcal{R}^2_{\rm T} \propto \sum^{3}_{i=1} (L_{ij} - L_{ik})^2.
\end{equation}
When the arm lengths are fully equal, the response to a GW signal could be canceled and make T channel as a quasi-null stream. However, in a realistic geodesic orbit, the arms to construct the TDI paths are not perfectly equal. In this scenario, the T channel can still respond to a GW signal even it could be $\sim$5 orders worse than X channels at the lower frequency as shown in Fig. \ref{fig:response_1st}. Since the response of X channel is proportional to $L^{2}$ at low frequency, this orders difference could be explained by the unequal arms from numerical orbit,
\begin{equation}
 \frac{\mathcal{R}^2_{\rm T}}{\mathcal{R}^2_{\rm X}} \simeq \frac{\delta L^2}{L^2} \simeq 10^{-5}.
\end{equation}
On the other side, the PSD of T channel is lower than X channels by $\sim$5 orders at $10^{-5}$ Hz as shown in Fig. \ref{fig:TDI1st_noise}.
Consequently, the sensitivity of T channel could be equivalent to X channel as shown in Fig. \ref{fig:Sensitivity_1st}.
There is a caveat that only acceleration and optical path noises are considered here in the PSD of T channel, the imperfect TDI due to path difference would upraise laser frequency noise, and further make sensitivity deteriorate. We commit ourselves to this study in the upcoming work \citep{Wang:2020ongoing}.
\begin{figure}[htb]
\includegraphics[width=0.48\textwidth]{./LISA_TAIJI_sensitivity_XUPD.eps}
\includegraphics[width=0.48\textwidth]{./LISA_TAIJI_sensitivity_XAET_EqualArm.eps}
\caption{\label{fig:Sensitivity_1st} The average sensitivities of selected TDI channels at starting time. The regular TDI channels (Michelson-X, Relay-U, Beacon-P and Monitor-D) are plotted in the upper panel, and optimal-A, E and T channels  with Michelson-X are shown in the lower panel. The sensitivity of T channel for fully equal arm configuration are shown by curves LISA-T-EqualArm and TAIJI-T-EqualArm, and this sensitivity is consistent with the T channel results described in \cite{Prince:2002hp,Vallisneri:2007xa}. (The curves of P and D channels are fully overlapped in the upper panel, as well as the A and E channel in the lower panel. The confusion noise is not considered in sensitivity estimations).}
\end{figure}

As the figures show, the average sensitivities of Beacon-P and Monitor-D channels are identical, as well as the pair of the optimal optimal-A and E channels. Even so, their instant antenna patterns and sensitivities to a same source could be different. Therefore, in the simulations included in the following two sections, the sensitivity of a TDI channel to a GW signal is calculated with variables including time, frequency, orientation and polarization, etc.

\section{Binary Supermassive Black Hole Mergers} \label{sec:SMBH}

The SMBH binary coalescence is one of the most important sources for LISA and TAIJI missions. In this section, we investigate the angular resolutions of LISA, TAIJI and joint network for the coalescing SMBH binary system.

\subsection{The source of SMBH binary}

LISA is expected to detect the SMBH binaries in the mass range of $10^5-10^7 M_\odot$ up to redshift $z \simeq 20$ \cite{2017arXiv170200786A}, as well as the TAIJI mission with the equivalent sensitivity. A mass ratio of $q=1/3$ is supposed to be the typical for these sources \cite{Colpi:2014poa}. Those coalescences could associate with the X-ray counterpart which could be detected by the Athena in redshift $z \lesssim 2$. \citet{Colpi:2019} investigated the sky localization of LISA for typical SMBH binary coalescences at the redshift $z=0.5,\ 1$ and $2$ which could trigger the efficient Athena follow-up observations.

TAIJI is expected to be launched in the 2030s and could have overlapped observation time with LISA and Athena. The joint observation of LISA and TAIJI could significantly improve the sky localization precision for the SMBH binaries \cite{Ruan:2019tje}. To quantify this improvement, referring to the assumptions in \cite{Colpi:2019}, the sources considered in our simulation are following, 1) $m_1 = 10^7 \ M_\odot, m_2 = 3.3 \times 10^6 \ M_\odot$, 2) $m_1 = 10^6 \ M_\odot, m_2 = 3.3 \times 10^5 \ M_\odot$ and 3) $m_1 = 10^5 \ M_\odot, m_2 = 3.3 \times 10^4 \ M_\odot$ in source frame at redshift $z = 2$. The GW observations are simulated for 30 days to the coalescences. The redshift effect on the GW waveforms are included by adopting the cosmological parameters from the Planck 2015 results \cite{Ade:2015xua}. The redshifted amplitudes of three optimal orientated sources in frequency-domain are shown in Fig. \ref{fig:SMBH_and_sensitivity}, as well as the averaged sensitivity curves of TDI channels.
\begin{figure}[htb]
\includegraphics[width=0.48\textwidth]{./LISA_TAIJI_SMBH_sensitivity_UnequalArm.eps}
\caption{\label{fig:SMBH_and_sensitivity} The amplitude of frequency-domain GW waveform from facing on/off three SMBH binaries at redshift $z=2$ and averaged sensitivity curves of (X, A, E, T) TDI channels at starting time. The GW signals start from the frequency at 30 days before the coalescences. }
\end{figure}

The approximant IMRPhenomPv2 is employed to represent the GW waveform which includes the inspiral-merger-ringdown phases \cite{Khan:2015jqa}. The LALSuite and PyCBC are utilized to implement the numerical waveform \cite{lalsuite,pycbc}. Eight parameters are considered to describe a GW signal with respect to the SSB coordinates which are ecliptic longitude $\lambda$, ecliptic latitude $\beta$, GW polarization angle $\psi$, inclination $\iota$, luminosity distance $D$, coalescence phase $\phi_c$, total mass of binary $M$ and mass ratio $q$. In our Monte Carlo simulation, the $(\lambda, \beta)$ is randomly sampled in the sphere, $\psi$ is uniformly sampled in $[0, 2 \pi]$ and $\cos \iota$ is sampled uniformly in $[-1, 1]$, and the starting time of GW signal is uniform in one year. 2000 binaries are generated for each kind of SMBH binaries.

\subsection{Fisher information matrix method} \label{subsec:FIM_FD}

The Fisher Information Matrix (FIM) is widely employed to determine the uncertainty of parameter measurements for GW observation \cite{1994PhRvD..49.2658C,Cutler:1997ta,Vallisneri:2007ev,Kuns:2019upi}. For multiple detectors, the joint FIM is calculated by summing up the FIM of each individual detectors,
\begin{equation}
\Gamma_{ij}  = \sum_{\rm det} \left( \frac{\partial h }{ \partial {\theta_i} } \bigg\rvert \frac{\partial h }{ \partial {\theta_j} }  \right)_{\rm det},
\end{equation}
with
\begin{equation}
\left( g | h\right)_{\rm det} = 4 \mathrm{Re} \int^{\infty}_0 \frac{g^{\ast} (f) h(f)}{S^{\rm det} (f) } \mathrm{d} f ,
\end{equation}
where $h$ is the GW waveform in frequency domain, $\theta_i$ is the $i$-th parameter measured, and $S^{\rm det} (f)$ is the noise PSD of one LISA/TAIJI TDI channel. From the FIM, the variance-covariance matrix of the parameters is obtained by
\begin{equation}
\begin{aligned}
\sigma_{ij} &= \left\langle \Delta \theta_i \Delta \theta_j  \right\rangle = \left( \Gamma^{-1} \right)_{ij} + \mathcal{O}({\rho}^{-1}) \overset{{\rho} \gg 1}{\simeq } \left( \Gamma^{-1} \right)_{ij} . \\
\end{aligned}
\end{equation}
For a detected source with a significant SNR ($\rho > 7$), the angular uncertainty of the sky localization is evaluated by
\begin{equation} \label{eq:delta_Omega}
 \Delta \Omega \simeq 2 \pi | \cos \beta | \sqrt{ \sigma_{\lambda \lambda} \sigma_{\beta \beta} -  \sigma^2_{\lambda \beta}  }.
\end{equation}

The TDI channels are treated as detectors to calculate the FIM individually and cooperatively.
The first-generation TDI configurations can make observation even when dysfunction happened in any two of the six laser links. When the full links are available, the three channels for each TDI configuration can operate simultaneously which can composite to three optimal TDI channels as shown in Eq. \eqref{eq:optimalTDI}. Four observation scenarios are considered in the simulation for a simulated GW signal: 1) only one regular TDI channel (X, U, P and D) of two missions is operating, (without losing the representativity, only one of three channels in each TDI configuration is included.), 2) optimal TDI channels (A, E and T) are available for a mission when full links are functional, 3) the joint observation of one mission's regular TDI channel with another's optimal TDI channels, and 4) the joint of two mission's optimal TDI channels.

\subsection{The results of sky localization}

The angular resolutions of LISA, TAIJI and joint network are evaluated by the described Monte Carlo simulations. For each simulated source, the uncertainties of the localization are calculated by Eq. \eqref{eq:delta_Omega} for the TDI channels, and their values are shown by cumulative histograms.
To represent the results concisely, we select the results of X, A, T and joint AET channels for a single mission, and results of one mission's AET with another's regular or AET channels for joint network.
Considering the field of view (FoV) of Wide Field Imager (WFI) on Athena is designed to be 0.4 deg$^2$ (40 arcmin $\times$ 40 arcmin) \cite{2013arXiv1306.2307N}, it would be rather easy for Athena's follow-up observation when the uncertainties are constrained in 1 deg$^2$.

The simulation results of $(10^7,\ 3.3\times 10^6)\ M_\odot$ binaries are shown in Fig \ref{fig:SMBH_m1_1e7}. The angular resolutions of TAIJI mission are slightly better than LISA in general. For the performance of individual missions, as shown in Fig \ref{fig:SMBH_m1_1e7} left panel, both LISA and TAIJI have lower angular resolution due to the relatively poor sensitivity in this corresponding band. Around $10\%$ and $20\%$ of the source could be constrained in 100 deg$^2$ by LISA and TAIJI's joint AET channels, respectively. The angular resolution of every single channel is closely identical due to their equivalent average sensitivities.
For the joint LISA-TAIJI observation, as shown in the right panel of Fig. \ref{fig:SMBH_m1_1e7}, we consider that a least one mission is in fully optimal TDI operation. When another mission is in TDI-X mode, more than $85\%$ of the sources could be localized in 1 deg$^2$. And all sources could be well localized in 0.4 deg$^2$ when both missions are in optimal operation.
\begin{figure*}[htb]
\includegraphics[width=0.48\textwidth]{./SkyLocation_m1_1e7_m2_3p3e6_z_2_AET_v3.eps}
\includegraphics[width=0.48\textwidth]{./SkyLocation_m1_1e7_m2_3p3e6_z_2_joint_v3.eps}
\caption{\label{fig:SMBH_m1_1e7} The histograms of sky localization uncertainties of LISA, TAIJI, and LISA-TAIJI network for $(10^7, \ 3.3\times 10^6 )\ M_\odot$ binaries at redshift $z=2$. The left panel shows the results of selected single (X, A, and T) and joint optimal (AET) TDI channels in individual missions, and the right panel shows the results of joint TDI channels in LISA and TAIJI missions. The channels from a single mission are denoted by mission-TDI. For the curves with label TDI-TDI, the first TDI label represent the channel of LISA, the second TDI label indicates the channel of TAIJI, e.g.  AET-X means the joint observation of LISA-AET and TAIJI-X channel.}
\end{figure*}

The simulation results of $(10^6,\ 3.3\times 10^5)\ M_\odot$ binaries are shown in Fig \ref{fig:SMBH_m1_1e6}. The left panel shows the histograms of selected TDI channels for individual missions. As we can read from the curves, the optimal AET channels can effectively improve the sky localization by around $1-2$ orders comparing to a single channel; $75\%$ and $50\%$ of the source could be localized in 1 deg$^2$ by TAIJI's and LISA's AET channels, respectively; the sky localization of optimal-T channel become worse than X and A channels due to its sensitivity bulge in the frequency band [0.5, 50] Hz.
The histograms of joint LISA-TAIJI observations are shown in the right panel of Fig. \ref{fig:SMBH_m1_1e6}. Following the same strategy, we keep at least one mission in optimal operation for joint observation. Although another mission's TDI-X mode degrades the localization ability comparing to the double fully optimal mode, all the joint the observation can constrain the source in 0.05 deg$^2$.
\begin{figure*}[htb]
\includegraphics[width=0.48\textwidth]{./SkyLocation_m1_1e6_m2_3p3e5_z_2_AET_v3.eps}
\includegraphics[width=0.48\textwidth]{./SkyLocation_m1_1e6_m2_3p3e5_z_2_joint_v3.eps}
\caption{\label{fig:SMBH_m1_1e6} The histograms of sky localization uncertainties of LISA, TAIJI, and LISA-TAIJI network for $(10^6,\ 3.3 \times 10^5)\ M_\odot$ binaries at redshift $z=2$. The left panels show the results of selected individual (X, A, and T) and AET channels, and the right panels show the results of joint TDI channels from two missions. TDI-TDI labels indicate the joint LISA (first TDI) and TAIJI (second TDI behind the dash) channels, e.g AET-X means the joint LISA-AET and TAIJI-X observation.}
\end{figure*}

The simulation results of $(10^5,\ 3.3\times 10^4)\ M_\odot$ binaries are shown in Fig. \ref{fig:SMBH_m1_1e5}. The left panel shows the histograms of TDI channels for individual missions. The optimal AET channels can effectively improve the sky localization by order(s) comparing to a single channel; almost all the sources could be localized in 1 deg$^2$ by TAIJI's and LISA's AET channels; the performance of optimal-T channel becomes much worse than X and A channels.
The histograms of joint LISA-TAIJI observations are shown in the right panel of Fig. \ref{fig:SMBH_m1_1e6}. Similar to the results of $(10^6,\ 3.3\times 10^5)\ M_\odot$ binaries, one mission's full optimal operation with another's TDI-X channel slightly decrease the localization performance compared to the double full optimal mode, all sources could be localized within 0.03 deg$^2$ by the LISA-TAIJI network.
\begin{figure*}[htb]
\includegraphics[width=0.48\textwidth]{./SkyLocation_m1_1e5_m2_3p3e4_z_2_AET_v2.eps}
\includegraphics[width=0.48\textwidth]{./SkyLocation_m1_1e5_m2_3p3e4_z_2_joint_v3.eps}
\caption{\label{fig:SMBH_m1_1e5} The histograms of sky localization uncertainties of the LISA, TAIJI, and LISA-TAIJI network for $(10^5, \ 3.3\times 10^4)\ M_\odot$ binaries at redshift $z=2$. The left panel shows the results of the individual (X, A, and T) and AET TDI channels, and the right panel shows the results of joint TDI channels from LISA and TAIJI missions. TDI-TDI labels indicate the joint LISA (first TDI) and TAIJI (second TDI behind the dash) channels, e.g AET-X means the joint LISA-AET and TAIJI-X observation.}
\end{figure*}

The performances of the individual TDI channels, more or less, could be reflected in Fig. \ref{fig:SMBH_and_sensitivity}, especially for optimal-T channel. For the SMBH binaries $(10^7,\ 3.3\times 10^6)\ M_\odot$ at redshift $z=2$, the frequency range in the 30 days coalescing is in $[0.04, 1]$ mHz where the T channel has the equal average sensitivity to detect GW signals to other TDI channels. The frequency range shifts to $\sim[0.15, 10]$ mHz for $(10^6,\ 3.3\times 10^5)\ M_\odot$ binaries. In this band, the detectability of the T channel starts to decline comparing to other channels. As for $(10^5,\ 3.3\times 10^4)\ M_\odot$ binaries, their frequency band changes to $[0.7, 80]$ mHz where the sensitivity of the T channel is much worse than others. Consequently, the ability of the T channel to detect and localize the sources becomes poor.

\section{Monochromatic Gravitational Waves Source} \label{sec:mono}

Monochromatic GW could be generated by compact binaries in the early inspiral and its frequency evolution is negligible in years of observation.
Galactic compact binaries containing a white dwarf or neutron star could emit quasi-monochromatic GWs in the low-frequency band which are detectable for the LISA and TAIJI. The GW signals from this population would overlap and form an unresolved foreground around a few mHz. Based on the different population assumptions, the foreground was evaluated in \cite{Nissanke:2012eh} and references therein. However, there are also known galactic binaries that could be resolved by space detectors, for instance, AM CVn (with an orbital period of $\sim$1000 seconds), HM Cnc ( $\sim$320 seconds) and V407 Vul ($\sim$570 seconds) \cite{Colpi:2019}. In this section, we investigate the angular resolution of the LISA-TAIJI network for the resolvable monochromatic sources.

\subsection{Fisher information method for monochromatic source}

The FIM formula is also employed to evaluate the uncertainties of sky localization for monochromatic sources. Considering there is almost no intrinsic frequency evolution (the observed frequency could be modulated with the detector's motion), the equations applied in Section \ref{subsec:FIM_FD} are not suitable for the monochromatic case. By using the Parseval's theorem applied in \citep{Cutler:1997ta,Vecchio:2004ec}, the FIM formula could be modified to
\begin{equation}
\begin{aligned}
\Gamma_{ij} &= \sum_{\rm det} \left( \frac{\partial h }{ \partial {\theta_i} } \bigg\rvert \frac{\partial h }{ \partial {\theta_j} }  \right)_{\rm det} \\
	&= \sum_{\rm det} \left[  \frac{4}{S^{\rm det} (f_0)}  \int^{\infty}_0 \partial_i h^\ast(f) \partial_j h(f) {\rm d} f  \right] \\
	&= \sum_{\rm det} \left[  \frac{2  }{S^{\rm det} (f_0)}  \int^{\infty}_0 \partial_i h(t) \partial_j h(t) {\rm d} t  \right].
\end{aligned}
\end{equation}
The waveform of a monochromatic signal is described by,
\begin{equation}
 h_{\rm} (t) = F^{\rm GW}_{\rm TDI} (f_0, t) \times \mathcal{A} \exp \left( 2 \pi f_0 t + \phi_0 \right),
\end{equation}
and the amplitude $\mathcal{A}$ of waveform in time-domain is \cite{Maggiore:2007}
\begin{equation}
 \mathcal{A} = \frac{4}{D} \left( \frac{G \mathcal{M}_c}{c^2} \right)^{5/3} \left( \frac{\pi f_0}{c} \right)^{2/3},
\end{equation}
where $F^{\rm GW}_{\rm TDI} (f_0, t)$ is the TDI response function at frequency $f_0$ and time $t$, $\phi_0$ is the initial phase, $D$ is the luminosity distance of the source, $\mathcal{M}_c = {(m_1 m_2)^{3/5} }/{(m_1+m_2)^{1/5}}$ is chirp mass and $c$ is the speed of light.
In this case, seven parameters are used to describe a monochromatic source which are longitude $\lambda$ and latitude $\beta$ of the source in SSB ecliptic coordinates, polarization angle $\psi$, inclination $\iota$, amplitude $\mathcal{A}$, initial phase $\phi_0$ and frequency $f_0$.

\subsection{Simulation and results for monochromatic source}

In the Monte Carlo simulation, the first step is to generate the sources in the galactic coordinate system and uniformly in a cylindrical volume with radial distance in [10, 50] kpc, azimuthal angle in $[0, 2 \pi]$ and height in $[-0.15, 0.15]$ kpc. Then the source locations are transformed to the SSB ecliptic coordinates by using the Python package -- Astropy (\url{https://www.astropy.org}). The amplitude $\mathcal{A}$ is generated assuming $m_1=m_2=1 \ M_\odot$. The polarization angle $\psi$ is randomly in $[0, 2 \pi]$ and inclination function $ \cos \iota$ is sampled uniformly in $[-1, 1]$. One-year observation is run with 1000 sources at frequency 3 mHz or 10 mHz. For comparison, we run an extra simulation at 10 mHz for the first 90 days observation.
In our current simulation, the sources are generated for the investigation of sky localization rather than specific for modeled galactic binary population.

To keep the estimations from FIM sensible, signals are removed when SNR from LISA-X or TAIJI-X channel is lower than 7 \cite{Vallisneri:2007ev}. The uncertainties of sky localization with SNR are shown in Fig. \ref{fig:Mono_SNR_SkyLocation}. The SNRs at 10 mHz is generally higher than SNR at 3 mHz due to the better sensitivity at 10 mHz than 3 mHz. And the sky localization is more precisely with the higher SNR. The bands formed by the detected signal in log-log plots trend to have the same slopes. As we can see the results from the first 90 days at 10 mHz which are shown by the markers with 90d, the single detector could localize the source with poor precision even with the same SNR comparing to 3 mHz. It could be due to the contribution of the Doppler modulation from orbit motion is largely missing. Even so, their LISA-TAIJI joint observation can improve the angular resolution by around one order. This may verify that the LISA-TAIJI network contributes more significant advantages to the short duration signals.
\begin{figure}[htb]
\includegraphics[width=0.48\textwidth]{./SNR_SkyLocalization_v2.eps}
\caption{\label{fig:Mono_SNR_SkyLocation} The sky localization uncertainties of the LISA, TAIJI, and LISA-TAIJI network with SNR for monochromatic sources. Three scenarios are included which are: 1) observing monochromatic wave at 3 mHz for one year (markers with @3mH); 2) observing monochromatic wave at 10 mHz for one year (markers with @10mH) and 3) observing monochromatic wave at 10 mHz for the first 90 days (markers with @10mH-90d). The AET-AET markers indicate the joint LISA-AET and TAIJI-AET observation results.}
\end{figure}

The histogram plots of localization uncertainties are shown in Fig. \ref{fig:Mono_SkyLocalization}.
TAIJI mission has slightly better resolution than LISA due to the better sensitivity. The detectability of TDI X and A channels are equivalent at both 3 mHz and 10 mHz. The joint observation can bring a relatively moderate improvement compared to a single LISA or TAIJI mission for one year observation.
For a given percentage, e.g. 80\%, LISA-AET channel (green solid line) could localize the sources at 3 mHz in $\sim 6.5$ deg$^2$, and joint LISA-AET and TAIJI-X channels, AET-X (pink solid line), can localize them within $3.5$ deg$^2$. The double optimal operations, AET-AET (yellow solid line), can constrain them in 2.3 deg$^2$. The joint observation also can improve the LISA-AET's angular resolution by 1 to 3 times in one-year observation for 80\% of the sources at 10 mHz.
For the percentages constrained in 1 deg$^2$, LISA-AET channel can localize the 20\% of simulated sources at 3 mHz, and AET-AET network can promote it to more than 50\%. For the sources at 10 mHz, almost all the sources could be localized within 1 deg$^2$ in one-year observation, and most of them could be localized in 1 deg$^2$ in the first 90 days by LISA-TAIJI network.
\begin{figure*}[htb]
\includegraphics[width=0.48\textwidth]{./SkyLocation_freq_3mHz_1yr.eps}
\includegraphics[width=0.48\textwidth]{./SkyLocation_freq_10mHz_1yr.eps}
\includegraphics[width=0.48\textwidth]{./SkyLocation_freq_10mHz_duration_90days.eps}
\caption{\label{fig:Mono_SkyLocalization} The histograms of sky localization uncertainties of the LISA, TAIJI, and LISA-TAIJI network for the monochromatic sources at 3 mHz (upper left panel) and 10 mHz (upper right panel) for one year observation, as well as at 10 mHz for the first 90 days observation (lower panel). The mission-TDI labels denote the results of channel from single mission. TDI-TDI labels indicate the joint LISA (first TDI) and TAIJI (second TDI behind dash) channels, e.g AET-X means the LISA-AET joint with TAIJI-X observation. }
\end{figure*}

The performances of TDI channels tend to identical for the channels with the equal averaged sensitivities at the corresponding frequency, as the X and A channels shown in Fig. \ref{fig:Sensitivity_1st}. The combined AET channel is effectively contributed by the optimal-A and E channels because of the poor sensitivity of the T channel at the 3 mHz and 10 mHz.
In addition, the amplitude of the monochromatic waveform is generated from assumed the galactic solar-mass compact binaries, and the FIM calculations take the amplitude as one parameter. Therefore, the results may represent simulations for more massive compact binaries from a larger distance as well.

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

In this work, we introduced the numerical orbit we achieved for LISA and TAIJI missions. To obtain the mission orbits, we employed an ephemeris framework to calculate S/C's geodesic including major gravitational interactions in the solar system. By implementing the orbital design and optimization workflow we created, the achieved LISA and TAIJI mission orbits could maintain in required status for 6 years without maneuver. And we assumed the starting time for LISA observation is on March 22nd, 2028 as a possible early schedule. If the observation starts from March 2030, there are still 4 years of valid mission orbit. If orbital maneuvers could be implemented, the orbit duration may be extended up to 10 years which could meet the LISA optimistic perspective \cite{2017arXiv170200786A}.

To understand the effects of TDI on GW observations, we examined four selected regulars (Michelson-X, Relay-U, Beacon-P, and Monitor-D) and three Michelson-type optimal (A, E, and T) TDI channels. We estimated the sky- and polarization- averaged sensitivities by using the current requirements on acceleration noise and optical path noise for LISA and TAIJI \cite{2017arXiv170200786A,Luo:2020}. And these sensitivities are time dependent and vary with the arm lengths. On the other hand, the calculations are based on the assumption that laser frequency noise is fully canceled by the first-generation TDI. However, the second-generation may be required for a realistic orbit to suppress the laser frequency noise under the acceleration and optical path noise \cite{Dhurandhar:2002zcl,Cornish:2003tz}, and their responses to GW could be depressed in this case especially for the lower frequency band \cite{Vallisneri:2004bn}. We would like to work on it in our future studies.

In order to investigate the angular resolutions of the LISA-TAIJI network, we run the Monte Carlo simulations for coalescing SMBH binaries and monochromatic sources. For each TDI channels, we calculated their response functions with variables including time, frequency, orientation, polarization, etc. For three SMBH populations at redshift $z=2$, $(10^7,\ 3.3 \times 10^6)\ M_\odot$, $(10^6,\ 3.3 \times 10^5)\ M_\odot$ and $(10^5,\ 3.3 \times 10^4)\ M_\odot$, the results showed the LISA-TAIJI joint observation significantly improve the angular resolution comparing to solo LISA or TAIJI mission. In an optimal scenario, all the simulated SMBH binaries could be determined in 1 deg$^2$ by the LISA-TAIJI network which would bring great merits for Athena's observations. The improvements are expected to take effect especially for short duration signals which are required to be identified quickly and precisely. Furthermore, we can deduce that SMBH binaries with comparable chip mass within redshift $z<2$ would be localized even more precisely. Another interesting result was shown by the detectability of the optimal-T channel to the SMBH binaries. With an irregular sensitivity curve comparing to the previous expectations \cite{Prince:2002hp,Vallisneri:2007xa}, its performance is rather different for the different masses binaries.

The GW waveforms for coalescing SMBH binaries are represented by the IMRPhenomPv2 approximant. And only dominant quadrupole ($(l, m) = (2, \pm2)$) modes are included in the simulation. The waveform with higher harmonics could substantially increase the angular resolution for smaller mass ratio \cite{2007PhRvD..76j4016A,2010PhRvD..81f4014M}. The newly developed higher mode PhenomHM with spin effect may worth applying to the smaller mass ratio in the future for the LISA-TAIJI network \cite{London:2017bcn}.

For the monochromatic sources in one-year observation, the improvement of angular resolution by the LISA-TAIJI network is relatively moderate compared to single LISA mission. The network can improve the localization by a factor of 2 to 4 for a selected percentage of sources because longer observation of a single mission is supposed to compensate the disadvantage and reach a certain accuracy comparing to the two detectors. For a shorter observation, for instance, 90 days we simulated, the network still represents a considerable advantage.

In our current simulation, the confusion-foreground noise from galactic binaries is not considered. We suppose the confusion noise can decrease SNR by a limited amount and bring an insignificant impact on the SMBH binary simulations. It may change the results to a certain extent for the monochromatic sources. However, at a given SNR, we suppose it would not significantly change the conclusions about the relative improvement of sky localization by the LISA-TAIJI network. Their joint observation may also help to resolve the confusion-foreground, and we commit it as another study in the future.

\begin{acknowledgments}
This work was supported by NSFC No. 11773059, Key Research Program of Frontier Sciences, Chinese Academy of Science, No. QYZDB-SSW-SYS016 and the Strategic Priority Research Program of the Chinese Academy of Sciences under grant Nos. XDA1502070102, XDA15020700 and XDB21010100. and by the National Key Research and Development Program of China under Grant Nos. 2016YFA0302002 and 2017YFC0601602.
This work made use of the High Performance Computing Resource in the Core Facility for Advanced Research Computing at Shanghai Astronomical Observatory. The authors would like to thank the anonymous referees for their valuable comments and suggestions.
\end{acknowledgments}

redpajama_set_name: RedPajamaArXiv


text:
RC Bhargava
Maruti Suzuki will grow in double digits in next three years: RC Bhargava
Speaking to shareholders at Maruti Suzuki's 36th annual general meeting, chairman RC Bhargava said the automotive industry largely reflects the changes in the economy
Ketan Thakkar
ET Bureau
September 06, 2017, 08:21 IST
Updated: September 06, 2017, 08:32 IST
Maruti Suzuki, India's largest carmaker, predicts the Indian automotive industry will grow in the double digits for the next three to five years, aided by conducive government policies though the pace of infrastructure development is a challenge.
Local unit of Japan's Suzuki Motor, which has outpaced the industry in growth in past several years, is also projecting double-digit expansion for itself.
Speaking to shareholders at Maruti Suzuki's 36th annual general meeting, chairman RC Bhargava said the automotive industry largely reflects the changes in the economy and that he is a firm believer that all the changes that are happening are going to facilitate much faster economic growth.
The company will grow in double digits in the next three years and meet its stated target of selling 2 million vehicles a year by 2020, he said.
Overall, the future of the industry is bright, though urban infrastructure could pose some problems, he said.
"Car buying will be curtailed by infrastructure challenges and the infrastructure growth may be comparatively slower than what we need to build. While highway infrastructure is growing, the urban infrastructure development is lagging behind in most part of India," said Bhargava.
The chairman is upbeat on Maruti Suzuki, which had a more than 51% market share in India in the April-August period, the first five months of this fiscal year. Bhargava said: "The growth of Maruti will certainly be in double digits and we should be able to achieve our target which we had set earlier of 2 million by 2020 and going further we have to now look into volumes of 2.5 million and 3 million."
He said with the support of parent Suzuki, which is investing, installing and operating a production facility in Gujarat, Maruti Suzuki has not only been able to increase profit but also almost doubled shareholder dividend payment.
The company will focus on automotive industry without getting deviated to other diversification plans, he said.
On queries of shareholders whether Maruti Suzuki should explore the defence space, which has now been opened up for private players, Bhargava said it need not divert attention from its core to do something new and need to focus on growth in the auto sector.
"There is a significant growth potential for the automotive sector and as a leader we need to play our part, whether it is in sales and service infrastructure, bringing in new technologies or fulfilling the aspirations of the Indian buyers with right products," he said.
Lauding the government's move on GST, Bhargava said it is a game-changer for the Indian industry and economy.
"It will still take some time (for benefits to show) because many structural changes will have to be made to enable this, but as the economy grows faster (as a result of GST) you will see that there is a spurt in demand for cars in this country," added Bhargava.
"The impact of GST is seen, there is a universal acknowledgement. Tax-on tax structure is gone, there is a greater compliance on tax payment and, lastly, there is a big benefit on the logistics front, which is a significant cost and affects the entire ecosystem," he said.
Over the past few decades, the Indian economy has become increasingly inconsistent in what is required to grow it into a modern industrial and competitive country and some of the reform measures taken by the government will help fix that, he said.
Maruti Suzuki growth
Auto industry growth
Business of Brands / 1 hour ago

redpajama_set_name: RedPajamaCommonCrawl


If you want to get a copy of the tools that I demonstrate in this video please click on this link and create an account. Once you have an account then click on this link to browse all of my databases, if you want, you can take a copy of the databases to use for yourself.
If you want to download any of the following views to a spreadsheet you can clock 'download CSV' to get your own private copy, or use the web based database I'm using by watching the video above.
For completeness here's a view of my master sowing database with all the details!
Watch out for the next video showing what I'm sowing in March!
Whereabouts in the country are you situated? I ask, because although I intend to follow your blog it might be wiser for me to make adjustments to take account of any difference in the ambient temperatures. Where I am now is about two weeks behind where I used to live and as a result lost a lot of my early seedlings last year.


WhatsApp Messenger is steadily getting popular as an alternative to the stock SMS service offered by many smartphones. With this app, you can send virtually unlimited text messages and even send photos or include emoticons for (almost) free. It works through 3G or WiFi.
The app is even ad-free so no annoyance while using it. It comes with a (little) price though. It would be free to download this App for Android and you can use it for only 1 year for free. Afterwards, you'll have to pay a $0.99 subscription fee to continue using it. The power of WhatsApp is in its large network. While the exact number of subscribers is not disclosed, Google play has recorded 1.2 billion downloads of the app (Skype has 650 million; Viber has 300 million). Furthermore, it is available for iOS, Nokia, Blackberry, iPhone, iPad and Windows phones. This app eliminates the need for a text plan which can significantly reduce expenses especially when messaging people from other countries.
WhatsApp is often compared to different pieces of messenger software, but comparing it to Hike has caused reviewers some difficulties because of how similar the two apps really are.
WhatsApp and Hike are both geared toward the same type of user, and both offer competitive options that many people use. This means that personal preference might have a lot to do with what choice individual users ultimately make.
WhatsApp has become a household name in recent years, but Kik has recently threatened to take away some of the market share this instant messaging giant carved out. Kik is growing by leaps and bounds.
Unlike apps like Hike or Line, Kik appeals to as wide a customer base as WhatsApp does. This has made it popular with those who are currently displeased with WhatsApp and have been looking for some kind of an alternative.


text:
UPDATED: Google Is Stopping Production Of The Pixel, Says Telus
Update: Google has responded to this story - see our edit at the end.
The Google Pixel and Pixel XL were only released in October, but according to a Canadian phone network, production is already stopping.
Softpedia reports that customers of the Telus network who'd ordered either of the phones got an email from the carrier letting them know they'd better pick a different handset:
"Please be advised that we have received notice today that Google will be ceasing production of their Google Pixel line and we will not be receiving further inventory of this phone. Therefore we will not be able to fulfil your order for the selected product. We apologize on behalf of TELUS and Google for this inconvenience."
Of course, this is only one source - but the Pixel XL in particular has been dogged by supply problems since release, and it's entirely possible other networks have had the same notification but didn't pass on the reason. The HTC-manufactured phone was well-received (when it was received), being awarded the highest-ever DxOmark score for a smartphone camera and being considered Android's answer to an iPhone by many - although not our reviewer.
If production has indeed stopped, it's likely that Google is gearing up for the Pixel's successor. Let's hope the Pixel XL 2 is a little easier to get hold of - in both senses.
Update: Google has provided a statement to 9to5Google:
We're really excited by the demand for the Pixel XL in Canada. Telus is currently out of stock of the Pixel XL. We're working with our partners to restock inventory across our retail channels and we can confirm that production of the Pixel has not stopped.
However, while the site says this refutes Telus' statement, technically it doesn't: the Telus email says "Google will be ceasing production" and Google's says "production has not stopped." Both of these things could be true, and it seems a bit strange for Telus to make that up and email it to a bunch of customers. So who's right? We'll see.


With more than 343,000 net square feet of exhibit space, the premier industry event has more to offer than any other industry trade show. Global Pet Expo takes place March 21-23, 2018 in Orlando, Fla.
The American Pet Products Association (APPA) and Pet Industry Distributors Association (PIDA) present the premier industry event, Global Pet Expo.
The Retailer Excellence Awards presentation takes place in the Valencia Ballroom at the Orange County Convention Center, Thursday, March 22.
The New Products Showcase Awards Presentation takes place on the Show Floor in the New Products Showcase section on Thursday, March 22.
With 84.6 million pet-owning households in the U.S., consumers continue to look for the latest and greatest the industry has to offer. Global Pet Expo is the first pet products trade show of 2018, and as the pet industry's largest annual show, it is an amazing opportunity for qualified media and buyers to see first-hand all the hottest and newest pet products before they hit store shelves.
Global Pet Expo 2018 will feature more new products and qualified buyers, All Under One Roof, than ever before! A qualified buyer attending Global Pet Expo works for an established business with a proven record of purchasing pet products from a manufacturer or distributor in quantity for resale to the consumer. Global Pet Expo has an unmatched qualification process that ensures buyers are attending this Show to make purchasing decisions and place orders with our exhibitors.
The 13th Annual Show, dubbed as The Show That Means Business, took place in March 2017, and featured 6,761 qualified buyers, 1,130 exhibitors and 3,437 booths sold – making for record-setting numbers. Total Show attendance came at 16,646, with 343,700 net square feet of exhibit space which was 24,000 feet larger than the 2016 Show. On a truly global front, 27% of exhibitors were international, making up 305 of the 1,130 exhibitors and more than 25% of buyers were from outside of the U.S., coming from 79 countries. In order to recognize the increase in international participants, the 2017 Show debuted country-specific pavilions which gave participating country delegations dedicated space throughout the exhibit floor. As the international participation has continued to grow, Global Pet Expo has once again proved itself as a key trading opportunity for companies from around the world.
Companies launching new products can highlight them in the New Products Showcase, where buyers and media have the opportunity to preview all the newest products hitting the industry in one convenient location. The 30,000-square foot space on the trade show floor is set aside to recognize the year's best creative efforts in New Product and Point-of-Purchase Displays. With nearly 1,000 entries submitted, this is the largest new products showcase at any pet product industry trade show in the world. The New Products Showcase "Best in Show" awards are the most coveted awards given in the industry. Winners will be announced at the Eighth Annual New Products Showcase Awards presentation. In order to be eligible to win, products must be entered in the New Products Showcase.
In addition to opportunities on the Show Floor, attendees can also attend the 2018 Global Pet Expo Academy. Managed by PIDA, the 2017 seminar lineup featured 29 different seminars from 16 expert instructors in the fields of marketing, social media and technology, merchandising, management, personnel and retail operations. Described by attendees as, engaging, insightful and informational, the 2017 Global Pet Expo Academy was a huge success with more than 1,600 attendees, a 23% increase over 2016.
The tremendous success of the continuously growing Global Pet Expo has been recognized by the trade show industry. Trade Show ExecutiveMagazine (TSE) ranked the Show #61 on their exclusive "Gold 100" list. This honor recognized Global Pet Expo as one of the 100 largest shows that "Set The Gold Standard" for the trade show industry, exceeding thousands of others in exhibit space, exhibiting companies and attendance. Global Pet Expo is also ranked #48 in TSE's Fastest 50 for fastest growing trade shows and was honored at the prestigious Trade Show News Network (TSNN) Awards as a Top 25 Fastest-Growing Show in net square footage.
There's no better place to experience the power of the pet industry than at Global Pet Expo! Global Pet Expo is open to independent retailers, distributors, mass-market buyers, and other qualified professionals, making it the most important gathering of buyers, pet product manufacturers, and international attendees in the U.S. The Show is not open to the general public.


The Cloudify pure-play orchestration platform provides a generic automation engine that spans the diversity of tools used in production environments from the apps through the networking services, databases and infrastructures. Through our role-based access control and fine-grained multi-tenancy – developers can have access to their applications, while IT remains in control of the resources and data.
Cloudify uses a declarative approach based on the TOSCA specification (Topology and Orchestration Specification for Cloud Applications), in which users focus on defining the desired state of the application through simple and readable terms, and Cloudify takes care of reaching the desired state all while continuously monitoring the application to ensure that it maintains the desired SLAs in the case of failure or capacity shortage.


text:
NHS England and NHS Improvement – East of England
NHS England and NHS Improvement – Midlands
NHS England Midlands and East
Missed GP appointments in the West Midlands costing NHS millions
More than one million general practice appointments are being wasted in the West Midlands each year because patients fail to turn up without prior warning.
There are around 22 million booked slots with GPs, nurses, therapists and other practice staff across the region every year and 5% of those are missed without enough notice to invite other patients – working out as around 1.1million wasted appointments.
Around 440,000 of these are with busy family doctors, which equals more than 73,000 GP hours wasted each year – the equivalent of 37 GPs working full time for a year.
Each appointment costs an average of £30, putting the total cost to the NHS at more than £33 million on top of the disruption for staff and fellow patients.
NHS England is working to improve access to GPs and other health professionals by recruiting thousands of new practice staff and appointments are now available in evenings and weekends in every general practice in the West Midlands.
Patients are also being encouraged to make use of GP online services, where they can book and cancel appointments, order repeat prescriptions, access some of their medical records and more. To register, simply take your ID to your practice and ask for the relevant forms.
However, it's vital patients do their bit by letting the NHS know if they cannot attend an appointment.
Dr Francis Campbell, Deputy Medical Director at NHS England West Midlands, said:
"We know that timely access to general practice appointments are a priority for the public, which is why we are growing the workforce and offering extended access. The NHS long term plan will set out how we build on this progress, but patients can do their part by letting their practice know as soon as possible if they can't make their slot – freeing up doctors, nurses and other professionals to see others. This is particularly important as we go in to winter."
Evening and weekend access to GP services has been available across the country since December, more than three months ahead of schedule, and means there will be an estimated nine million extra appointments each year. They are available across seven days and through designated local NHS services, or in some cases a patient's own GP practice.
Professor Helen Stokes-Lampard, Chair of the Royal College of GPs, said:
"When patients miss appointments it can be a frustrating waste of resources for GPs and our teams, but also for other patients who are struggling to secure an appointment for themselves.
"There may be many reasons why a patient might miss an appointment, and in some cases it can be an indication that something serious is going on for that individual – but we would urge patients to let us know if they can't attend as soon as possible, so that we can offer that time to someone else who really needs it. To this end, practices are using electronic methods, such as SMS reminders, to encourage patients to keep their appointments, or cancel them in a timely manner."


SolarWinds.Data.SWQL.SWQLSyntaxException: mismatched input 'RETURN' expecting 'FROM' ---> Antlr.Runtime.MismatchedTokenException: A recognition error occurred.
notice that in each count, you have to name the column inside the expression (renamed as n) in order for it to be accepted.
Is it possible to make these numbers clickable, so that we can see which are these devices ?


text:
/ Xeni Jardin / 1:05 pm Fri Mar 29, 2013
Bollywood Easter: Images of Christ in '70s poster art from India
My brother Carl Hamm (Twitter), who is a club and radio DJ and a collector of obscure but excellent global stuff, shares the images in this post and says:
There's a long tradition of Indian poster art which was probably at its height in the 1970s but goes back many many years before then. Youve already seen vivid and colorful posters for Hindi films.
Often the same artists who were painting "pinup" style posters of bollywood heros and heroines were also painting similarly colorful calendar and poster art of gods, goddesses, politicians, national heros, etc.
The artists' subjects were diverse and sometimes included icons of the west -- including Jesus as seen here. (Ive also seen posters of Kennedy)
Poster artists would also paint advertisements for perfume, bicycle manufacturers, beedi vendors, health tonic, insurance companies and banks, political campaigns, car batteries, makeup and feminine hygiene products.. and would incorporate the same lavish style in the ads for these ordinary products -- and often include either a film star or even a religious deity on the same advertisement.
It was also common for religious posters like these to have a calendar (sometimes with rotating wheels with the date) and a company name.
I'm currently reading a great book on the subject of Indian poster art called Gods in the Bazaar.
Since today is Good Friday, I'm sharing a few interesting depictions of Jesus; I'm sharing others as examples of the other diverse subject matter these artists were painting for calendars, ads, and "inspirational pinups".
Some of the studios/artists here include: JB KHANNA AND CO (Madras aka Chennai) "Jesus life,"
S.J BRIJBASI AND SONS "Holy Family", and STUDIO SVARAS, "Jesus with arms outstretched."
(Source: random piles of stuff on the internet. Artists unknown, alas.)
art / bollywood / easter / folk art / india / indian / pop art / religion
Al Jaffee's MAD Life: how a traumatized kid from the shtetl became an American satire icon
Back in 2010, It Books published Mary-Lou Weisman's biography of MAD Magazine icon Al Jaffee: Al Jaffee's Mad Life: A Biography; I missed it then but happened upon Arie Kaplan's 2011 writeup in The Jewish Review of Books this morning and was charmed by the biographical sketch it lays out.
The flags of Russia's regional governments are amazing
From Zheleznogorsk's flag depicting a bear splitting an atom (the city started as a plutonium mining-town) (yours for $60!) to Domnovskoye's stark eagle claw to Syaskelevskoe's drunken bull to Khoroshyovo-Mnyovniki's crudely drawn MS-Paint-style proud beaver, the flags of Russia's states, cities, towns and districts are pretty fabulous; Weird Russia has a giant trawl through them. […]
There's a particle accelerator in the Louvre's basement
Three basement levels of the Louvre are given over to the Centre de recherche et de restauration des musées de France (C2RMF), which provides research and restoration services to France's 1,200+ art museums and galleries.


The cause for the increase primarily falls on the shoulders of Republic Airlines and the company's decision to take on extra route responsibilities without having crews to man those flights.
Republic is one of three carriers that operates aircraft under the United Express banner at the Durango-La Plata County airport.
Crew shortages on Republic flights were the main cause of a twofold increase in delays and cancellations on United Express flights between October and December, said Jodi Doney, the Skywest/United Express Station Manager during a January presentation to the Durango-La Plata County Airport Commission. Controllable delays rose from 16 percent to 32 percent from October to December while controllable cancellations jumped from 2.5 percent to 5.6 percent, Doney told the commission.
"They're spreading themselves fairly thin," she said of the airline.
Republic's problems are rooted in the carrier's decision to take on another contract with United Express that was previously held by Colgan Air. Colgan was phased out of operation in September after its parent company, Pinnacle Airlines Corp., filed for Chapter 11 Bankruptcy Protection in April 2012 .
According to a May news release, Republic purchased about 30 aircraft from Colgan Air and began operating the planes in August. The transition went smoothly at first, but as Republic took on additional routes to places such as Gunnison, Grand Junction and Eagle, the company fell behind on hiring and training crews to staff the new aircraft and fly the new routes, Doney said.
The problem probably won't start to improve until March, Doney said.
"Hopefully, they will start to recover by our spring break," she said.
Calls made to Republic Airlines for comment were not returned.
Despite the hassles for La Plata County fliers, Brockus complimented Republic Airlines and United Express for relaying information about the cause of recent delays and cancellations.
Expressjet and Skywest also operate aircraft flying in and out of La Plata County under the United Express label, but the "vast majority" of significant nonweather-related issues were on flights operated by Republic Airplanes, Brockus said.
Airline flight ratings bear out that statement. Between Nov. 15 and Jan. 15, almost 70 percent of the flights from Denver to Durango operated by Republic were rated poor or very poor based on on-time performance, while 19 percent of those operated by Skywest and 28 percent operated by ExpressJet were poor or very poor, according the website flightstats.com.


text:
JESUS & DRUMPF
NON-SPORTS TALK
14 dead, 50 injured by lone gunman in Batman premiere in Colorado
By big_dish
July 20, 2012 in JESUS & DRUMPF
Lewdog
[quote name='Fulcher_33' timestamp='1342832031' post='1139953']
When I read these arguments I can't help but laugh. For some reason it seems as if the people that are for more people carrying guns actually believe that if a gunman came in shooting up a place that they would just pull out their firearm and defuse the situation. This ain't Hollywood, boys. I'm not saying you wouldn't defend yourself but let's be real, you'd be shitting yourself if some fucker with an automatic weapon came in shooting the place up. On top of that, especially in this theater shooting, it was fucking dark and people were going crazy trying to get out of there. In my opinion, if there were these "5 people with permits" sitting there it would have been so easy for one of them to shoot one of the others by mistake. You don't know which one is the gunman, all you see is someone with a gun in a room full of panic. Also, someone said that if there were 5 law abiding people in there that were allowed to carry, and if one of them was up front, that he could have taken the guy out or at least slowed him down. Well sure, if you're going hypothetical on us then anything is possible. Fact of the matter is this, there could have been 50 people in there with CCW permits and none of them may have been up front. And if we're going to be hypothetical then we might as well just say that this could have been prevented if they had better security on their damn doors. You know, this guy was wearing a bulletproof vest. If someone in the front row had stood up and shot at him I can almost guarantee that that person would have ended up in a body bag.
Look, I'm not 100% against people owning guns. I grew up in rural Kentucky and there were guns in my house since I was born. I'm fully trained to use a gun. I do feel that there needs to be much much much stricter gun laws though. And yes, I'm against CCW. I wouldn't be comfortable walking down the street knowing that at any moment one of these law abiding CCW holders may have had a bad day at work, after a big fight with the wife, and he just decides to take it out on some others. Fuck you guys acting like everyone with a CCW can't have something happen to them that makes them snap. People walking around with guns is a huge, huge mistake.
Oh yeah, someone mentioned that if there were more CCW permits would it possibly deter shit like this from happening? I think not at all. The death penalty sure as shit hasn't deterred anyone. Prison hasn't deterred too many from committing crimes. People like this fucking idiot that shot up the theater are not right in their fucking head to begin with. You actually believe that they would be of sound enough mind to think about the downside to what they're doing and decide not to do it?
There are good arguments on both sides, within reason. Fact of the matter is this, there are too many guns in America now that it would be impossible to clean it up and get rid of them. It's something that you guys have to live with.
To be totally honest, now that I sit back and REALLY think about it, instead of stricter gun laws I'd like to see people learn to treat others with a little more respect. That alone would drop the crime rate down a hundred fold. I do believe the old NRA saying that "Guns don't kill people, people kill people" and America is a fucking cesspool when it comes to respecting your fellow man. That is an entirely different argument though.
MULLY
Mully that Death Penalty argument is actually a poor one. In Texas where they don't just sentence people to the death penalty, but actually USE it, they have lower crimes rates than other similar states.
T-Dub
BENGALS FANATIC
[quote name='Lewdog' timestamp='1342842843' post='1139984']
In Texas where they don't just sentence people to the death penalty, but actually USE it, they have lower crimes rates than other similar states.
What similar states?
Homer_Rice
[url="http://www.deathpenaltyinfo.org/murder-rates-nationally-and-state"]Just in reference to murder, this does not seem to be true.[/url]
|Elflocko|
Elflocko
|GB ELITE SUPPORTER|
Location:Prague, Czech Republic
[url="http://www.texastribune.org/library/data/fbi-crime-statistics-2010/"]Yeah, not so much... [/url]
|Lucid|
|GB MOD TEAM|
Location:Westwood
Seriously Dish, a lot of this stuff you are repeating sounds a lot like lobbyist talking point propaganda.
[quote name='Homer_Rice' timestamp='1342844021' post='1139987']
[quote name='Elflocko' timestamp='1342844713' post='1139988']
[url="http://www.texastribune.org/library/data/fbi-crime-statistics-2010/"]Yeah, not so much...[/url]
[url="http://www.deathpenaltyinfo.org/murder-rates-nationally-and-state#MRalpha"]http://www.deathpena...d-state#MRalpha[/url]
So at 5 murders per every 100,000 Texas does pretty darn good for being on the boarder with Mexico and dealing with gang violence and immigration. There are a lot of factors other than just the Death Penalty.
There are 17 other states with a higher murder rate than Texas.
Just FYI Colorado only had 2.4 murders per 100,000 people in 2010.
So at 5 murders per every 100,000 Texas does pretty darn good for [b]being on the boarder with Mexico and dealing with gang violence and immigration[/b]. There are a lot of factors other than just the Death Penalty.
You're right, forgot about all them Mexicans... Point made sir! I'm guessing the 17 states with higher murder rates also had more Mexicans.
[quote name='big_dish' timestamp='1342832426' post='1139954']
Even with body armor, a .40 or .45 would knock him back, or knock him completely over.
That's simply not true. Again it seems that your ideas on this subject in general are based on video games and/or action movies. There are plenty of articles debunking the myth of "stopping power" or energy transference, but here's one of them:
http://www.firearmstactical.com/briefs3.htm
Note in particular the real-world examples from law enforcement of heavier, higher velocity rounds than would typically be used for CCW's failing to incapacitate even an [i]unarmored[/i] assailant. Watch the video from the "North Hollywood Shootout" for a more immediate demonstration of how meaningless "stopping power" is against a person in body armor.
[quote name='Lucid' timestamp='1342855183' post='1139996']
There are Mexican drug cartels right across the border leaving human heads on downtown streets....some of this drug violence has spilled over into towns like Brownsville. There is nothing racist about what I said, it's the truth.
Total truth.. Especially when you consider all these "immigrants", they outnumber the drug dealers and gang members 10 maybe 20 to 1 easy.. It's amazing Texas has such low murder rates. Only 17 states with higher you say?
Jamie_B
Location:VA
I agree with this [url="http://video.msnbc.msn.com/hardball/48264648#48264648"]Reagan[/url]
big_dish
Location:Ft Lauderdale Beach
[quote name='T-Dub' timestamp='1342855418' post='1139997']
[url="http://www.firearmstactical.com/briefs3.htm"]http://www.firearmst...com/briefs3.htm[/url]
What? This case study says nothing about knocking someone back or knocking someone over. It has to do with incapacitation and death by placement/arterial disruption. I said nothing about that. You arent getting hit with a large round and not getting the energy transfer- often its the reaction to the bullet hitting the armor that causes the body to react/stumble/fall/disorient momentarily. It would be like someone jabbing you hard with the end of a broomstick- it is a sudden, forceful impact. I didnt mention anything about penetrating torsos/necks/arteries.
I feel the same way about what you are saying- because I dont agree with it. You dont agree with me so you feel that way.
So, to summarize:
Shooting people: Had it coming.
Shooting birds: Cruel.
[img]http://www.hchs.hunter.cuny.edu/wiki/images/d/d3/LOLWUT_Pear.jpg[/img]
Yeah its weird that humans have this odd thing that allows them to reason and make cognitive decisions and the ability to foresee the impact those decisions may have on the future. Animals dont. So when humans make decisions such as rape/robbery/assault/murder, they get whats coming to them sometimes. Virtually all animals are innocent, so to speak.
MichaelWeston
Go-Bengals.com Content Contributor
[quote name='T-Dub' timestamp='1342841163' post='1139980']
In that case man you're just being squeamish and really don't have a leg to stand on.. Not saying you need to go out and hunt a cow or anything, but complaining about hunting when you're probably eating meat from factory farms? Fresh fish & game is far less cruel.. and [i]much[/i] tastier, too.
I don't disagree. For me it's entirely the act of seeing something alive and then snuffing out its life for sport and kind of food if you made me kill my chicken or cow I would be a vegetarian
|kennethmw|
kennethmw
Location:dayton, oh
My beef with the whole "gun control" debate, is that for the most point we talk around each other. Dish, I don't want to take your guns, I have a few myself. My problem is with assault rifles and high capacity magazines. I don't think either should be allowed. Dish, a CCW holder in the situation as described, probably would have made it worse, however, a CCW holder being there with him only having a 10 shot magazine might have been able to prevent a number of Deaths/Injuries. Personally, as a Hunter, I see no reason for the high capacity magazines, and it seems that in most of the major disturbances, they have been HUGE contributors to the loss of life and or Injuries sustained.
Ron~Popeil
[quote name='Jamie_B' timestamp='1342807659' post='1139893']
Saw this on one of the comedian's I follow's FB.
Dear Internet People,
Maybe choose another day day to make pro gun statements.
Both sides should tone it down. Nothing says shitty American politics like using a tragedy to make political points before the bodies are even buried.
sois
Did this dude have mental issues?
This shooting was probly unpreventable. You can't prepare for random. Shit happens.
PS reminded me of this song:
[url="http://www.youtube.com/watch?v=TdbrxHLhOn8"]http://www.youtube.com/watch?v=TdbrxHLhOn8[/url]
[b]I feel the same way about what you are saying[/b]- because I dont agree with it. You dont agree with me so you feel that way.
Really? Like what? Maybe you are attributing other posters statements to me?
What? This case study says nothing about knocking someone back or knocking someone over.
Um.. That's what "kinetic energy transfer" means.
[quote][font="Arial"][size="3"][color="#000000"]There's not one documented incident in which an officer was knocked unconscious or physically incapacitated or in any way rendered unable to perform willful activity after his soft armor stopped such a projectile. These officers absorbed nearly 100 percent kinetic energy transfer, yet [b]none were incapacitated by the blunt trauma "shock" of projectile impact[/b] or temporary displacement of underlying soft tissues.[/color][/size][/font][/quote]
|Bunghole|
Location:Bright, Indiana
Or you could, you know...shoot him in the head.
[quote name='Bunghole' timestamp='1342909754' post='1140069']
That's surprisingly hard to do actually in good circumstances.. You know from your training in the military you are taught to shoot center mass, because aiming for the head likely means a miss. I qualified "expert" with the M16A2, so I do have some experience with this (missed 50m target because I jerked).
He was also wearing a helmet.
Virtually all animals are innocent, so to speak.
Again, unless you're a vegetarian I'm really not interested in your views on "innocent animals".
|Numbers|
I was taught double tap to center mass with one to the head. Close quarter drills were different as compared to what a qual range for a rifle or pistol were. Aiming for the head is a difficult shot regardless of whether it is close range or long range, especially so if firing under duress. However, if you or anyone else has hit someone at center mass twice already and they are still standing, it makes sense to try a head shot to stop the bad guy.
[quote name='Numbers' timestamp='1342963198' post='1140128']
The Navy I was in taught me that if I hit the ocean 10 times using a .45 without ripping any of my digits off via the retraction of the slide, then I was good to go!


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