text:
Q: Change Angular Timepicker font size I'm using the angular bootstrap timepicker but I cannot seem to change the font size which cuts off some of the text like below:

HTML:

                End:
                <timepicker ng-model="filter_endtime" ng-change="changed()" hour-step="hstep"
                    minute-step="mstep" show-meridian="ismeridian"></timepicker>

If I inspect the element in a browser I can change the .form-control font-size to 12px and it looks fine.
.form-control {
    display: block;
    width: 100%;
    height: 34px;
    padding: 6px 12px;
    font-size: 14px;
    line-height: 1.4285;
    color: #555;
    background-color: #fff;
    background-image: none;
    border: 1px solid #ccc;
    border-radius: 4px;
    -webkit-box-shadow: inset 0 1px 1px rgba(0, 0, 0, .075);
    box-shadow: inset 0px 1px 1px rgba(0,0,0,0.075);
    -webkit-transition: border-color ease-in-out .15s, box-shadow ease-in-out .15s;
    transition: border-color ease-in-out .15s, box-shadow ease-in-out .15s;
}

Is there anyway I can override the font size in the timepicker control?
I've tried doing
font-size: 12px !important;

as another class in the input-group but it makes it look like this:

A: change .form-control class styles in your bootstrap css.
.form-control{
font-size:12px
}

or use inline style
<timepicker style="font-size:12px;" ng-model="filter_endtime" ng-change="changed()"
hour-step="hstep" minute-step="mstep" show-meridian="ismeridian">
</timepicker>

A: Just set css for .bootstrap-timepicker-hour and .bootstrap-timepicker-minute:
bootstrap-timepicker-hour{
font-size:12px !important;
}

Try in fiddle
http://jsfiddle.net/sqe64a09/


text:
Another member for the AVnu Alliance
Yamaha has become the latest Promoter Member of the increasingly high-profile organisation that aims to support and promote AVB networking standards.
By David Davies
The decision means that companies in the wider Yamaha group – including Nexo S.A. and Steinberg Media Technologies – can also be involved in the Alliance.
Established in August 2009, the AVnu Alliance has expanded rapidly in line with the emergence of AVB (audio-video bridging) as a leading topic of debate across the pro-audio world. From a line-up of founder members comprising Broadcom, Cisco Systems, Harman International , Intel Corp, Samsung Electronics and Xilinx, the Alliance has announced a slew of new Promoter Members, with the most recent additions including Analog Devices, Barco, Pelagicore, Shure and Biamp.
With the addition of Yamaha, the organisation now has a grand total of 19 Promoter Members in addition to its six founders.
Although it will be "maintaining support for existing open-format protocols", Yamaha said that its decision to join the AVB-promoting AVnu Alliance reaffirmed its "dedication to providing users with the most up-to-date, flexible system solutions through products that will support AVB in addition to current network technologies."
"Our customers require a common network platform from all manufacturers," said Larry Italia, vice- president/general manager, Yamaha Commercial Audio Systems, Inc. "Yamaha products 'speak any language', and as a market leader in digital formats, we have much to contribute to these standards as we have with our other third party platforms."
Lee Minich (pictured), AVnu Alliance marketing workgroup chairman and president of Lab X Technologies, remarked: "We are very pleased that Yamaha has joined the AVnu Alliance. They are a significant force in live and commercial installed audio applications, and joining the AVnu Alliance, confirms that Audio Video Bridging–enabled devices will play an important role in the future direction of the commercial A/V industry."
www.avnu.org
www.yamahacommercialaudio.com
AVnu Alliance welcomes new member Axon and forms Pro Video subgroup
AV-IT
AVnu Alliance announces expansion into industrial market
AVnu Alliance welcomes new member
Biamp joins AVnu Alliance
AVnu Alliance unveils new certification logo
Crestron joins AVnu Alliance
Dolby Laboratories joins AVnu Alliance
Barco, Shure among new AVnu Alliance members

redpajama_set_name: RedPajamaCommonCrawl


Shoppingholics & Zoyou - I must be lucky this month! | Memorable Days : Beauty Blog - Korean Beauty, European, American Product Reviews.
Shoppingholics & Zoyou - I must be lucky this month!
EEEEK! I must be lucky this month since I won two giveaways xD: Circle lenses from Shoppingholics.com and a pair of earrings from Zoyou.nl.
Anna hosted a giveaway for Shoppingholics a month ago, where the winner could win an EOS or Candy magic circle lenses. Believe it or not, I was the one who won that giveaway !!! AAAAH ='D So, I went to the shoppingholics website and chose a pair of EOS lenses that I wanted. I chose the EOS adult blue circle lenses (E-203BL), which is from their old serie. After a week or so I received the lenses and whoa, the first thing what I said was: "Super cute x3"! Yes, the packaging was super cute!
It came along with a cute card and a piggy lens case ^__^.
I've always wanted to have blue lenses !! I haven't tried these on yet ^^ but I'm going to review them soon =D!
Besides the circle lenses I also won a pair of earrings. It was from a Zoyou giveaway which was hosted by Tasja. The winner could win a pair of bow earrings ^___^. Well, here they are, aren't these cute =3 ?!
Like I said, it's my lucky month hahaha! What's next =p? LOL!
Ah leuk, ben benieuwd hoe die lenzen je staan!
Ah ze zijn leuk ^^! Ben benieuwd hoe ze je staan :D!
the packaging is so cute! Please have the reviews soon :D:D Have a great weekend!
Gefeliciteerddd ik wil weten hoe die lenzen jouw staan!
Very good choice ;) You'll love the blue Adults!!
haha you lucky babe! i love the earrings!
ooo you are lucky~ I can't wait to see how you look with blue lens!
:OOO oh quite lucky!! Everything is so cute~ How are you liking the lenses? They're a pretty style!
Wow what great luck! Can't wait to see you with the lenses on!
aah, die strikjes zijn leuk!
I got the same from Solution-Lens.com if you know.


Walk through our doors and take a step back in time. Every room overflows with 1920s period detail, from real tin ceilings to authentic carpet patterns, to high tank toilets in the rest rooms. The four main spaces are the Bar, Casino, Cabaret, and Lounge, connected by a network of secret pass-throughs, hallways, ramps, and chambers. Entrance to the venue is only through one of our false-front businesses, Joe's Clock Shop or Sam Lee Laundry. In the bar, our cocktail menu features world-class recreations of classic Jazz Age concoctions, all made from the finest modern ingredients.
In the 125-seat Cabaret, we offer top-notch Vaudeville-style entertainment, drawn from the immersive theatre hit "The Speakeasy". Customize your own line-up featuring our dance chorus, chanteuse, comedy duo, ventriloquist, sword swallower, jugglers, magicians, aerialists, and burlesque artists. Our 4-6 piece house band keeps the joint jumping with a knock-out jazz repertoire. The Casino features black jack, craps, and roulette, on our custom-built 1920s gaming tables -- "for entertainment only" -- staffed by expert dealers in period costume.
Our most popular event format starts with a cocktail hour and appetizers in the Bar, followed by a 45-minute Vaudeville show in the Cabaret. You've already got the crowd's attention, so following the show is the perfect moment for the host to take the stage for a special announcement, awards presentation, or just to say thank you. Next, the party moves to the Casino and Bar, for an hour or two of gambling, spirits, and general merriment. But the possibilities expand from there. We'll work with you to combine elements and create your perfect event format. Film screening, dance floor, photo booth, even sit-down meals are all possible. With our partner Exit Reality we can even incorporate a virtual reality experience into the evening, if you really want your guests to time travel!


text:
Home Politics Hassan Ayariga says the appointment of Charlotte Osei as chairperson of the...
Hassan Ayariga says the appointment of Charlotte Osei as chairperson of the electoral commission is President John Mahama's worst mistake.
Think Ghana
Disgruntled flagbearer of the All People's Congress Hassan Ayariga says the appointment of Charlotte Osei as chairperson of the electoral commission is President John Mahama's worst mistake.
"What did Charlotte Osei do when she was head of the NCCE? She failed in everything she did there, and now she has been appointed chairperson of electoral commission; and she has the guts to disqualify me for what she failed to educate us on.
"In fact, Mr President, I look you in the face and tell you that her appointment is the worst mistake so far," angry Ayariga told a news conference in Accra Friday.
He said the EC chair is targeting him unfairly, citing the claim by Mrs Osei that "Hassan Ayariga will not win the elections" during an address in the UK.
According to him, inasmuch as he would want to contest his disqualification in court, he would not want to do anything to frustrate the upcoming polls.
Ayariga was disqualified by the Electoral Commission again after the Supreme Court had ordered that some 13 disqualified presidential candidates be given the opportunity to correct the errors on their nomination forms.
He and seven others were rejected on Wednesday after the chairperson of the election management body said subscribers on their list did not meet the requirement by law.
Ghana goes to the polls on December 7, to elect a president and Parliamentarians.
President Mahama and the NPP's Nana Akufo-Addo are the frontrunners in the polls watchers expect to be close.
Source:Ghana/StarrFMonline.com/103.5FM/Kwame Danso Acheampong
#Hassan Ayariga says the appointment of Charlotte Osei as chairperson of the electoral commission is President John Mahama's worst mistake.
Previous articleNana Addo Dankwa Akufo-Addo, is calling on all Ghanaians to vote for their future on December 7, stressing that the poverty and hunger that have engulfed the country under President Mahama are no respecter of tribe or ethnicity.
Next articleProf. Kwamena Ahwoi has cautioned the Zongo communities not to fall for the "lies and deception" of the opposition New Patriotic Party (NPP)
Ghanaians have no hope in politicians like Joshua Akamba- Koopong Dankwah
Amb. Victor Smith lobbies to be Mahama's running mate for 2020
Vivian Abla Kpeglo; best choice for NDC Deputy National Organizer position


text:
\section{Introduction and Summary}

The detection of gravitational waves (henceforth GW) and the onset of the new field of gravitational-wave astronomy is one of the most exciting challenges for science in the XXI century, completing what is sometimes alluded to as Einstein's Unfinished Symphony. The detection of GW will open a new window onto the universe, that in addition to revealing exciting information on exotic systems such as black holes or cosmic strings is expected to also unravel as yet unexpected sources.

One of the interesting sources for low--frequency GW are the so called I(E)MRI sources, or Intermediate (Extreme) Mass Ratio Inspirals. Those are the GW emitted by a system including a smaller compact object whose orbit decays into a much larger massive black hole (MBH). Typical sources are stellar mass black holes inspiraling into a supermassive black hole, like those residing at the center of galaxies, and also IMBHs (intermediate mass black holes) inspiraling into MBHs. The importance of such sources is that because of the extreme mass ratio  the smaller compact object can be viewed as a test particle, thus probing the spacetime of the larger black hole and its surroundings. {\it Inter alia}, such sources will allow us to test directly the Kerr hypothesis, and allow us to map the spacetime surrounding such exotic objects. Moreover, the detection of I(E)MRIs will allow us to determine the mechanisms that shape stellar dynamics in galactic nuclei with unprecedented precision \cite{Amaro-Seoane2012}.

The orbits of I(E)MRIs are typically highly relativistic, and exhibit exciting phenomena, e.g.~extreme periastron and orbital plane precessions. Because the orbital evolution time scale (``radiation reaction time scale'') is much longer than the orbital period(s), over short time scales the orbit is approximately geodesic, yet on long time scales it deviates strongly from geodesic motion of the background. Instead, the smaller objects moves along a geodesic of a perturbed spacetime. Alternatively, one may construe the orbit as an accelerated, non-geodesic motion in the spacetime of the unperturbed central object, where the acceleration is caused by the self force (henceforth SF) of the smaller object \cite{Poisson-Pound-Vega}.

Detection and parameter estimation of GW from  I(E)MRIs relies on the construction of theoretical templates. A number of approximation schemes for such templates are available. Firstly, the energy balance approach (``the radiative approximation'') uses balance arguments for otherwise conserved quantities, and relates the flux in these quantities to infinity and down the event horizon of the black hole with the particle's orbit, so that the latter can be adjusted to agree with the fluxes \cite{Hughes}.
As the orbital evolution time scale is typically much longer than the orbital period(s), the radiative approximation is very satisfactory during the adiabatic phase of the motion. As the particle's orbit is affected by the fluxes away from it, when the orbit is not stationary one encounters complex retardation effects.
Most currently--available EMRI waveforms have been obtained by such an approach. This approach, however, ignores conservative effects that do not register in the constants of motion.

These retardation effects are completely avoided when one considers a local approach to orbital evolution in terms of the SF. (One should bear in mind, however, that the SF itself is a non-local quantity, with contributions arising from the quasilocal neighborhood of the particle and possibly beyond \cite{Anderson}.) In addition, the local approach to the calculation of orbital evolution via the SF is not restricted to the adiabatic regime, it avoids the complications associated with the rate of change of the Carter constant, and, most importantly, it includes also conservative effects that are discarded when one uses balance arguments. Over the last decade much progress has been made in the computation and understanding of the SF in General Relativity (for recent reviews of the self force in General Relativity see \cite{Poisson-Pound-Vega,barack:2009}).

The computation of the fully relativistic SF allows one to include conservative effects in the waveform templates, and study the importance of the conservative effects. True self consistent orbit and waveforms include the instantaneous solution of the coupled SF integrated equations of motion and the perturbation equations, or equivalently the interaction of the particle with its own field over its half--infinite past world line \cite{gralla-wald}. Very recently, for the scalar field toy model, such self consistent Schwarzschild orbits and waveforms were presented \cite{diener}.
Here, we are making the simplifying assumption that the effects of the difference between the SF that is calculated for the actual orbit (the self consistent approach \cite{Pound,gralla-wald}) and that which is calculated for a geodesic of the same instantaneous orbital parameters, is smaller than the effects of the latter and hence negligible at first order. This approximation is valid for as long as the orbital evolution is adiabatic, that is as long as the orbital evolution time scale is much longer than the orbital period(s). In a Schwarzschild background of mass $M$, the adiabatic approximation holds when the mass ratio $\eta:=\mu/M$ is such that $\varepsilon\gg \eta^{1/2}$, where $\varepsilon$ measures the distance to the innermost stable orbit, specifically $\varepsilon=p-6-2\epsilon$ where $p$ is the semilatus rectum and $\epsilon$ is the orbital eccentricity \cite{cutler}.  In practice, our approximation is to a leading order in $\eta$ beyond geodesic motion. We neglect terms that are linear in second--order SFs, although our method is amenable to their inclusion when they become available. This approximation is valid for at least a part of the relevant parameter space \cite{burko04}, but as their inclusion would contribute linearly to the dephasing, the contribution of the conservative piece of the SF (hereafter CSF) may be isolated as is done here.
Using true self consistent waveforms will both produce more accurate waveforms, and allow us to test the accuracy of this approximation. Most importantly, our approach allows us to see for the first time the effect of the CSF on GW emitted from IMRI sources.

We present here the first waveforms obtained with inclusion of the CSF, and study its effect within the simple class of quasi--circular orbits around a Schwarzschild black hole.  Specifically, we study the effect of the system's mass ratio on the dephasing that occurs when one neglects the CSF. We find weak dependence of the dephasing on the mass ratio, in accord with expectations based on the scaling of the number of orbits with the inverse of the mass ratio, and the scaling of the dephasing effect of the CSF per orbit with the mass ratio. We also find that the dephasing depends quadratically on the initial point of the motion for the range of parameters we tested.
We reiterate that second--order dissipative effects are ignored in this Paper. Their inclusion will guarantee the full consistency of the model, and will be comparable to the self-consistent approach. The inclusion of the second-order dissipative effects awaits further development to both theory and computational techniques.

The organization of this Paper is as follows: In Section \ref{method} we discuss the computational and numerical methods that we use. In Section \ref{results} we discuss our results for the orbits (\ref{orbit}), the waveforms (\ref{waveform}) and the dependence of the dephasing on the mass ratio and the initial point of the motion (\ref{varying}).

\section{Method}\label{method}

We use the fully relativistic SF obtained by Barack and Sago \cite{Barack-Sago} for circular Schwarzschild geodesics to drive the orbital evolution (our computation allows for an easy replacement with a different force expression, say one that includes second order dissipative effects, or spin--orbit coupling effects when becoming available), and compare the resulting waveforms with those obtained from the energy balance approach and those obtained when only dissipation is left in the SF, setting by hand the CSF to vanish. In practice, we consider a point source $\mu$ in a quasi--circular orbit around a Schwarzschild black hole $M$ with a mass ratio $\eta:=\mu /M$, and the motion starts at  a value of the semilatus rectum $p_0$ until it gets close to the ISCO at $p=6$. Such sources are relevant to the NGO capabilities: NGO will have the capability to detect GW emitted by an IMBH in the mass range $10^{2-4}M_{\odot}$ spiraling into a MBH in the mass range $3\times 10^5-10^7M_{\odot}$ such that the mass ratio is $10^{-3}-10^{-2}$ out to cosmological redshift $z\sim 2-4$. In addition, advanced LIGO could detect compact stellar sources spiraling into an intermediate mass black hole (IMBH) in the same mass ratio range \cite{brown:2007}. We specialize below to this mass ratio range, $\eta\in [10^{-3}-10^{-2}]$. Although the linearized  approach used here is intended to be used only when $\eta\ll 1$ and one may not simply extend the range of $\eta$ to high values and still expect accurate results, the error involved from neglecting $O(\eta^2)$ terms in the self force (specifically its dissipative piece) is comparable to the accuracy of our computation. In this sense, to within the accuracy of our numerics, we are justified in studying the IMRI case as long as we do not raise $\eta$ beyond $10^{-2}$.

We integrate the equations of motion using the Barack--Sago SF which was calculated for momentary circular geodesics. As the Barack--Sago SF is tabulated for a select choice of orbital radii, we interpolate to intermediate values such that the original accuracy is maintained. Specifically, we match two asymptotic expansions: at large distances (which we take in practice to be $r>8M$) we take the standard post--Newtonian expansion for the luminosity in gravitational waves, and construct from it the temporal component of the SF. To 5.5 PN order the PN expression does not provide us with sufficient accuracy to reproduce all the $r\ge 8M$ data points of the Barack--Sago data. We therefore add an effective remainder term that appears like a 6PN term, and fit its two free parameters to agree with all the large distance tabulated data to all significant figures. The radial component, or CSF, is modeled by a PN--like expansion with four free parameters. At short distances we expand the SF such that convergence is fast and only four free parameters are needed for either component. Specifically, we expand the radial component about the ISCO, the Innermost Stable Circular Orbit at $p=6$. The expansion functions are as follows:

 \begin{eqnarray}
f^t_{r\le 8\,M}&=&-
\frac{1}{\sqrt{1-\frac{3M}{r}}\left(1-\frac{2M}{r}\right)} \; \bigg(\frac{M}{r}\bigg)^5\; \bigg(\frac{\mu}{M}\bigg)^2\;
\Bigg[a^-_0\nonumber\\
&+&a^-_1\,\frac{M}{r}+a^-_2\,\bigg(\frac{M}{r}\bigg)^2+a^-_3\,\bigg(\frac{M}{r}\bigg)^3 + \cdots \Bigg]
\end{eqnarray}
\begin{eqnarray}\label{pn}
f^t_{r\ge 8\,M}&=&-
\frac{32}{5}\,\frac{1}{\sqrt{1-\frac{3M}{r}}\left(1-\frac{2M}{r}\right)} \;\left(\frac{M}{r}\right)^5\;\left(\frac{\mu}{M}\right)^2\\
&\times&\;
\left[ {\rm PN}_{5.5}+\left(a^+_6+a^+_{6L}\,\ln\frac{M}{r}\right)\left(\frac{M}{r}\right)^6 + \cdots \right]\nonumber
\end{eqnarray}
\begin{eqnarray}
f^r_{r\le 8\,M}&=&
\bigg(1-\frac{2M}{r}\bigg)\; \bigg(\frac{M}{r}\bigg)^2
\bigg(\frac{\mu}{M}\bigg)^2\nonumber\\
&\times&\;
\Bigg[b^-_0+b^-_1\,\bigg(1-\frac{6M}{r}\bigg)+b^-_2\,\bigg(1-\frac{6M}{r}\bigg)^2\nonumber\\
&+&b^-_3\,\bigg(1-\frac{6M}{r}\bigg)^3 + \cdots\Bigg]
\end{eqnarray}
\begin{eqnarray}
f^r_{r\ge 8\,M}&=& \bigg(\frac{M}{r}\bigg)^2
\bigg(\frac{\mu}{M}\bigg)^2\;
\Bigg[b^+_0\\
&+&b^+_1\,\frac{M}{r}+b^+_2\,\bigg(\frac{M}{r}\bigg)^2
+b^+_3\,\bigg(\frac{M}{r}\bigg)^3 + \cdots\Bigg]\nonumber
\end{eqnarray}
where ${\rm PN}_{5.5}$ stands for the standard $\frac{11}{2}$--post--Newtonian expression (converting Eq.~(3.1) in \cite{tanaka:1996} from luminosity to $f^t$ -- see Appendix \ref{PN}). Fitting the free parameters, we find the values appearing in Table 1.
\begin{table}[htdp]
\caption{The fit parameters for the self force. These parameters reproduce the accuracy of \cite{Barack-Sago} to all significant figures for all data points. Our results for $a^+_{6,6L}$ are very inaccurate predictions for the corresponding PN parameters, as our fit ignores all higher--order terms.}
\begin{center}
\begin{tabular}{|c|c||c|c||c|c||c|c||}\hline\hline
$a^-_0$ & 4.57583 & $a^+_6$ & 331.525 & $b^-_0$ & 1.32120 & $b^+_0$ & 1.999991\\
\hline
$a^-_1$ & 31.8117 & $a^+_{6L}$ & -2081.57 & $b^-_1$ & 1.2391 & $b^+_1$ & -6.9969\\
\hline
$a^-_2$ & -267.250 & & & $b^-_2$ & -1.297 & $b^+_2$ & 6.29\\
\hline
$a^-_3$ & 1049.27 & & & $b^-_3$ & 1.07 & $b^+_3$ & -24.6\\
\hline\hline
\end{tabular}
\end{center}
\label{default}
\end{table}%

The simplicity of our model allows us to easily separate the CSF effects. Specifically, for quasi--circular Schwarzschild orbits we may write
$f^{\rm SF}_{\mu}=
f^{\rm SF}_{t}
\,\delta^t_{\mu}+f^{\rm SF}_{\varphi}\,\delta^{\varphi}_{\mu}+f^{\rm SF}_{r}\,\delta^t_{r}$ where the last term on the right hand side (RHS) is purely conservative, and the first two are purely dissipative. We may therefore study the conservative effects by turning off by hand the last term on the RHS.

We integrate the SF driven orbit using two independent methods: one method is the osculating orbit approach \cite{Pound-Poisson} [specifically Eqs.~(43)--(47) therein], with special care given to the requirement that the orbit is quasi--circular. Specifically, free evolution may take the orbit away from quasi--circularity because
integration using the osculating geodesics method cannot keep the value of the eccentricity as precisely zero. As both variables $\alpha$ and $\beta$ (see \cite{Pound-Poisson} for definitions) are dynamical, the eccentricity $\epsilon$ must evolve along the orbit too. This behavior is shown in Fig.~\ref{alpha_beta}. Interestingly, the inclusion of the conservative piece of the self force amplifies the resulting eccentricity.

\begin{figure}[h]
 \includegraphics[width=7.5cm]{orbit4_bw.eps}
\caption{The osculating--code variables $\alpha$ and $\beta$ as functions of the time $t$ (upper two panels), and the effective eccentricity $\epsilon$ of the orbit (lower panel) as a function of $t$ in the osculating case. We show the results from the osculating orbits method with the inclusion of the CSF (solid curves) and with turning off the CSF (dotted curves). In all cases shown here $\eta=10^{-2}$ and $p_0=10$.}
\label{alpha_beta}
\end{figure}

The second method is the direct integration of the orbit. The direct integration method takes the local equation of motion to be $u^{\beta}\,\nabla_{\beta}u^{\alpha}=\mu^{-1}\,f^{\alpha}_{\rm SF}$ (``Newton's second law,'' with covariant differentiation compatible with the background metric) and integrates its solution. Both codes are numerically stable and convergent. Specifically, the osculating code converges with 5$^{\rm th}$ order, and the direct code converges with $4^{\rm th}$ order (Fig.~\ref{fig_conv}).

Comparing the two independent methods for finding the SF driven waveforms is not trivial because of a difficulty in finding identical initial conditions. Specifically, the osculating method requires as initial data only the specification of the initial position vector, which in our case is taken to be a circular geodesic at some initial $p_0$. The direct method, however, requires both the position and the velocity vectors to be specified, such that the constraint equation $u_{\mu}u^{\mu}=-1$ is also satisfied. The main difficulty is that in the initial data for the osculating method the initial $u^r_0=0$, such that it corresponds to an incorrect initial radial velocity for the direct method. In practice, we find the initial data for the direct code by generating the orbital parameters at $p_0$ by running the osculating code from some $p\gg p_0$ down to $p_0$, and then take the position and velocity vectors at $p_0$ as the initial data for the direct method. The residual disagreement in the initial data can be controlled to be compatible with our numerical error tolerance.  We then use the obtained orbits to generate the waveforms using a code for the sourced Teukolsky equation with hyperboloidal slicing, a code which converges at 2$^{\rm nd}$ order \cite{code}.

\begin{figure}
 \includegraphics[width=7.5cm]{conv_c.eps}
\caption{Convergence tests for the two codes. Top panels: the 4-position (A) and 4-velocity (B) for the osculating code as functions of the azimuthal angle $\varphi$. Lower panels: the 4-position (C) and 4-velocity (D) for the direct code and a function of time $t$. In all cases shown here $\eta=10^{-2}$ and $r_0=10M$, and the CSF is included.}
\label{fig_conv}
\end{figure}

As noted above, our approximation holds only for as long as $\varepsilon\gg \mu^{-1/2}$. We therefore do not integrate the equations of motion in practice all the way down to the ISCO at $p=6$, and stop the integration at a finite distance from the ISCO. In practice, we stop the integration at $p_{\rm final}=6.15\pm0.10$. Stopping at $p_{\rm final}$ is enough to estimate the dephasing at the ISCO: the dephasing $\,\Delta\Psi$ is a smooth function of the time $t$ along the particle's world line. In practice, we extrapolate $r$ as a function of $t$ to the ISCO to determine the time at which the particle arrives at the ISCO, and then we extrapolate the phase of the waveform to the same value of the time to estimate the phase of the waveform when the particle arrives at the ISCO. We may then find the difference of the total phases between two waveforms to find the dephasing $\,\Delta\Phi$.

\section{Results}\label{results}
\subsection{The orbit}\label{orbit}

We next choose $\eta=10^{-2}$ and $p_0=10$. There is of course nothing special about this choice of the parameters,  except that we couldn't make a much higher choice for $\eta$ and  justify it  with the linearized approximation used. Below we study the dependence of the effect on the parameters $\eta,p_0$.
The orbit is displayed in Figs.~\ref{orbit1},\ref{orbit2},\ref{orbit3} and \ref{orbit4} for the three codes. Notably, the two independent self force codes reproduce the orbit to high level of agreement, with a difference much smaller than the difference between either and the orbit generated in the energy balance approach. This difference is attributed to the effect of the conservative piece of the self force.

\begin{figure}[h]
 \includegraphics[width=7.5cm]{four_pos_new_bw.eps}
\caption{The Orbit. The 4--position for three orbital evolution codes: energy balance (dotted), direct evolution (dashed), and osculating code (solid).}
\label{orbit1}
\end{figure}

\begin{figure}[h]
 \includegraphics[width=7.5cm]{four_v_new_bw.eps}
\caption{The Orbit. The  4--velocity  for three orbital evolution codes: energy balance (dotted), direct evolution (dashed), and osculating code (solid).}
\label{orbit2}
\end{figure}

\begin{figure}[h]
 \includegraphics[width=7.5cm]{new_orbit_c.eps}
\caption{The Orbit. The shape of the orbit for the three orbital evolution codes: energy balance (dotted), direct evolution (dashed), and osculating code (solid). }
\label{orbit3}
\end{figure}

\begin{figure}[h]
 \includegraphics[width=7.5cm]{new_orbit_section_c.eps}
\caption{The Orbit. The shape of the orbit for the three orbital evolution codes: energy balance (dotted), direct evolution (dashed), and osculating code (solid). A small portion of the orbit shown in Fig.~\ref{orbit3} is magnified to show detail.}
\label{orbit4}
\end{figure}

The orbit, of course, is a gauge dependent quantity. Indeed, the position vector changes trivially under gauge transformations, $x^{\mu}\to x^{\mu}+\xi^{\mu}$. We can, however, create gauge invariant quantities in a specific gauge choice (in our case, the Lorenz gauge), and then those quantities are guaranteed to remain unchanged in any other gauge. Two independent gauge invariant quantities are $u^t$ (``gravitational redshift", ``helical Killing vector of the perturbed spacetime") and the angular frequency $\Omega$ \cite{detweiler:2008}. In Fig.~\ref{gaugeinv} we plot $u^t$ as a function of $\Omega$ with and without the conservative piece of the self force. Notably, to the accuracy of our numerical computation the two curves overlap. That is, we find -- as expected -- that $u^t$ as a function of $\Omega$ is insensitive to the conservative piece of the self force \cite{barack:2009}. This conclusion implies that when an actual data stream is used and this gauge invariant figure is plotted, one may use a simplified radiation--reaction scheme, that does not include the conservative effects in its analysis.

\begin{figure}
 \includegraphics[width=7.5cm]{gauge_inv_bw.eps}
\caption{The gauge invariant figure of $u^t$ as a function of the angular frequency $\Omega$. The curve without (dashed, $\circ$) and with the conservative effects  (solid, $\square$) are shown, together with equal-$t$ increment marks starting at $t=1,500\,M$ (at the bottom left) in increments of $1,000\,M$. The two curves are indistinguishable to the numerical accuracy of our computation (using the osculating orbits code in both cases).}
\label{gaugeinv}
\end{figure}

There is, however, an aspect of the gauge invariant figure (\ref{gaugeinv}) that is sensitive to the conservative effects, specifically the speed with which the data point moves along the curve. The way the conservative effects are manifested in the gauge invariant plot is not is the shape of the curve, but in the time it takes the signal to move along it. One may therefore observe the CSF effect by monitoring the motion of the data point representing the system along its curve on the $u^t-\Omega$ plane.
We note that one additional effect of the CSF is the shift in the ISCO \cite{barack-sago:2009}, which we do not consider here.

\subsection{The waveforms}\label{waveform}

We show the waveform for the case that the CSF is turned off in Fig.~\ref{fig1} for the same parameters discussed above, specifically $p_0=10$ and $\eta=10^{-2}$. We find that the waveforms obtained with the SF keeping only its dissipative pieces (and turning off its CSF) overlap with the energy balance waveform. Notice that the two waveforms in the figure are indistinguishable. The calculation method is very different in these two cases: In the SF case the orbital evolution is local; the orbit evolves because of a local force acting on the particle; in the energy balance case the fluxes to infinity and down the event horizon are calculated, and then the energy escaping over a period of the orbit is removed from the particle, and a new orbit with the new values of the constants of motion is found. The agreement of the waveforms is therefore a non-trivial test of the correctness of the calculation. The two waveforms overlap nearly exactly, with total cumulative dephasing at the order of $10^{-3}$ radians.

\begin{figure}
 \includegraphics[width=7.5cm]{figure1_c.eps}
\caption{The real part of the waveform $\psi_4$ when the CSF is turned off (solid), and using the energy balance approach (dashed, $\circ$).
The SF waveform was calculated with the orbit evolving using the osculating method \cite{Pound-Poisson}.}
\label{fig1}
\end{figure}

We next reintroduce the CSF. We integrate the SF driven orbit using two independent methods: the osculating orbit approach and direct integration of the orbit. Figure \ref{fig2} shows the waveform for the energy balance approach (same as in Fig.~\ref{fig1}) and for the two independent methods of calculating the SF driven orbit (including the CSF). The latter two waveforms are in agreement with each other with small dephasing (see below) between them, and a much larger dephasing of either with the energy balance waveform.

\begin{figure}[h]
 \includegraphics[width=7.5cm]{all_waves.eps}
\caption{The real part of the waveform $\psi_4$ when the CSF is included (solid for the osculating orbit method, and dashed for the direct integration method), and using the energy balance approach (dotted). The three waveforms are in phase at the beginning of the waveforms, but the former two dephase with time from the latter (and to a much smaller extent from each other).}
\label{fig2}
\end{figure}

The waveform dephasing of Fig.~\ref{fig2} is shown explicitly in Fig.~\ref{fig3}. We find that the total cumulative dephasing of the waveforms at the endpoint of the evolution at $p_{\rm final}$ is $\,\Delta\phi=10.3\pm0.4$ radians. The error estimate comes from the numerical errors in each calculation method and from residual incompatibility of initial data in the two SF driven cases, which we estimate by comparing the waveforms obtained from the osculating orbit approach and the direct integration approach.

\begin{figure}
 \includegraphics[width=8.0cm]{dephasing_new_c.eps}
\caption{The dephasing of the waveforms for the same data shown in Fig.~\ref{fig2}. We show the dephasing from the energy balance waveform of the waveforms obtained from both methods to calculate the orbital evolution when the conservative effects are included, and the dephasing of the two latter methods from each other.  Dashed curve:
dephasing of the waveforms from the osculating orbit method from the energy balance method; Dotted curve: dephasing of the waveforms from the direct integration method from the energy balance method; Thick solid curve: the average dephasing of the waveform. Dash--dotted curve: The difference between the dotted and dashed curves.
Insert: same as in the main figure, with the extrapolated dephasing down to the ISCO shown in a thin solid curve.}
\label{fig3}
\end{figure}

The dependence of $\,\Delta\Phi$ on the position $p$ is a simple monotonic unction of the time (Fig.~\ref{fig3}) which we can extrapolate from $p_{\rm final}$ down to the ISCO at $p=6$. We find that at the ISCO the dephasing is $\,\Delta\Phi=14\pm 1$ radians.
Dephasing of $14\pm 1$ radians corresponds to about $2.2$ cycles over the entire motion of the particle over 107.8  cycles. We next consider the following simulation of a detection event. Say the actual data stream is modeled by the waveforms obtained with the full SF expression, i.e., including the CSF, and that the theoretical template is obtained by turning off the CSF, or equivalently by using the energy balance waveform. By how much is the overlap integral of the waveforms reduced because of our ignorance of the CSF?

\begin{figure}
 \includegraphics[width=7.0cm]{C_of_t_c.eps}
\caption{The local overlap integral for a window of length $L=350M$ (dash-dotted) and of length $L=820M$ (solid) taken from the energy balance waveform and a piece of equal length of the full SF (including conservative effects) waveform obtained from the osculating orbit method, as a function of the starting point of the latter. The window is taken here from the end of the waveform (the late chirp part). The global maximum of the overlap integral is 0.9900 (for $L=350M$) and 0.9594 (for $L=820M$).}
\label{fig4}
\end{figure}

Figure \ref{fig4} shows the overlap integral as a function of the time, when we take a window of length $L$ of the energy balance waveforms (specifically from their late chirp part), and shift it along the waveform of the full SF. At each point we calculate the overlap integral of the window with a local piece of the second waveform, and plot the local overlap integral as a function of the start time of the window. Because the window was taken from the late part of the waveform, we find that the overlap integral is very small at first, and becomes large only at the late part of the other waveform. We then take the maximum of the overlap integral to be the one corresponding to the chosen window $L$.  More precisely, we calculate
$C_{\rm max}={\rm max}_{\tau}\,\frac{<\psi^{\rm SF}(t) | \psi^{\rm EB}(t-\tau)>}
{\sqrt{<\psi^{\rm SF}(t) | \psi^{\rm SF}(t)><\psi^{\rm EB}(t) | \psi^{\rm EB}(t)>}}\, .$
Larger values of $L$ would reduce the overlap integral even further. In Fig.~\ref{fig5} we show $C_{\rm max}$ as a function of the window size $L$.
As $L$ increases, at some value $C_{\rm max}$ would drop below a pre-determined value that marks our tolerance for detection or parameter estimation. Many times this threshold is taken to be $C=0.96$, because then detection rate would drop by $10\%$. Here, this threshold is obtained when $L_{\rm threshold}=816.6\,M$, which corresponds to just over 14 wavelengths of the emitted GW. If $L\gtrsim L_{\rm threshold}$, the exclusion of the CSF effects would cause a significant drop in the $C_{\rm max}$ that would reduce the detection rate by $10\%$ or more.  In such a case ignoring the CSF would have an important effect on detection or parameter estimation of the GW. However, short waveforms (i.e., $L < L_{\rm threshold}$) do not require the CSF effects to be included if reduction of the detection rate by less than this tolerance is acceptable.
The overlap integral increases rapidly as the template window is taken from earlier times.
This result suggests that when other parts than the very end  of the waveform is of interest, the full SF is even less significant than we have found.

\begin{figure}
 \includegraphics[width=7.0cm]{diff_win1.eps}
\caption{The maximal overlap integral for windows of varying length $L$ taken from the energy balance waveform and a piece of equal length of the full SF (including conservative effects) obtained from the osculating orbit method, as a function of the starting point of the latter. The circles are data points, and the curve is the quadratic fit
$C_{\rm max}=1.0010-1.7988\times 10^{-5}\,L-3.9154\times 10^{-8}\,L^2$, with fit parameter $R^2=0.9983$.}
\label{fig5}
\end{figure}

\subsection{Varying the values of parameters}\label{varying}

Our model of quasi--circular Schwarzschild orbits depends on two variables: the mass ratio $\eta$ and the start point $p_0$. Here we vary each parameter independently and find the dependence of the dephasing $\,\Delta\Phi$ [between the osculating orbits case (that includes the CSF) and the energy balance case (that neglects the CSF and considers only dissipative effects)] on either parameter.

\subsubsection{Varying the mass ratio $\eta$}

First we study the variation of the dephasing with changing the parameter $\eta$, the mass ratio. The greatest problem with varying $\eta$ is its effect on the computation time. On the one hand we cannot justifiably increase $\eta$ beyond $10^{-2}$, because then the linearization approximation breaks down. On the other hand, lowering $\eta$ to very small values, while satisfying the linearization requirement more confidently, results in longer physical evolution times and correspondingly also longer computation times.

In practice we reduce the value of $\eta$ by a full order of magnitude, and sample values in the range $[10^{-3}-10^{-2}]$, and fix $p_0=8$. (We decrease the value of $p_0$ from its previous value of 10 to save on computation time for the lower values of $\eta$.)

\begin{figure}
 \includegraphics[width=7.0cm]{dephasing_final_c.eps}
\caption{The dephasing $\,\Delta\Phi$ as function of time for a family of mass ratios $\eta$ for the values (from right to left): $\eta=$0.001, 0.002, 0.003, 0.005, 0.006, 0.007, and 0.010 (solid curves). The circles display the extrapolated values when the particle arrives at the ISCO, and the dashed line shows their average at $1.726\pm 0.021$. In all cases the motion starts at $p_0=8$.}
\label{fig6}
\end{figure}

Figure \ref{fig6} shows a family of curves displaying the dephasing between the cases of the osculating orbits method  and the energy balance method.
Each curve in Fig.~\ref{fig6} ends at the point we stop the integration when the orbits gets too close to the ISCO for the adiabatic approximation to still hold. These curves are very smooth and simple functions, which we extrapolate to the times at which the particle arrives at the ISCO. The extrapolated value of the dephasing at the ISCO is also shown in Fig.~\ref{fig6}.  We find only little variation in the dephasing as $\eta$ changes over a full order of magnitude, consistent with the expectation that the dephasing has only a weak dependence on $\eta$. Indeed, one could expect from scaling arguments that the dephasing per orbit scales with $\eta$ while the number of orbits scales with $\eta^{-1}$ (both scalings are indeed found in our simulations --- see Fig.~\ref{fig7}), so that the total dephasing is at the leading order at $O(\eta^0)$. Here we show that not only is the dephasing at $O(1)$, but in the range tested and with our numerical resolution is indistinguishable from a constant value, or at the most is a very weak function of $\eta$.

\begin{figure}
 \includegraphics[width=7.0cm]{dephasing_comparison_c.eps}
\caption{Five dimensionless quantities (denotes collectively by $N$) as functions of the mass ratio $\eta$: $\mu T/M^2$ (divided by 10 to keep the scale similar with the other four quantities) ($\diamond$), the dephasing $\,\Delta\Phi$ ($*$), the difference in arrival time $\,\Delta T/M$, and $\eta\Phi$ for the energy balance case ($\square$) and the osculating orbits case ($\circ$). Here, $\,\Delta\Phi$ and $\,\Delta T/M$ are between the osculating orbits and the energy balance cases, and $T$ is the total time of motion from $p_0$ down to the ISCO.  In all cases the motion starts at $p_0=8$ and the values shown are extrapolations to the ISCO.}
\label{fig7}
\end{figure}

In Fig.~\ref{fig7} we show five dimensionless quantities constructed from the evolution time $T$ from $p_0$ down to the ISCO, the total phase of the waveform in the energy balance and osculating methods case (including the CSF term), and the differences in arrival time and the dephasing between the latter two. We find that $T\sim O(\eta^{-1})$, that $\,\Delta\Phi\sim O(\eta^{0})$, $\,\Delta T/M\sim O(\eta^{0})$ and that in  both the energy balance and osculating orbits cases the total phase $\Phi$ is a linear function of $\eta$ with a very small slope, that is at the magnitude of our computational error. We therefore cannot rule out that we see in addition to the leading $O(\eta^{-1})$ term also a higher-order $O(\eta^{0})$ term. Notice that the last four quantities are comparable to each other, and that the variation in all five (at the most $10\%$) is very small compared with the full order of magnitude variation in $\eta$.

\subsubsection{Varying the initial position $p_0$}

Next we fix the mass ratio $\eta$ and vary the starting point of the motion $p_0$. In practice we choose the value of  $\eta=10^{-2}$. Figure \ref{fig8} shows the dephasing between the osculating orbits case (that includes the CSF) and the energy balance case (that neglects the CSF) for the range $p_0\in[8,10]$. Naturally, the dephasing grows with $p_0$. The data presented are consistent a quadratic dependence of $\,\Delta\Phi$ on $p_0$.

\begin{figure}
 \includegraphics[width=7.0cm]{dephasing_distance_c.eps}
\caption{The dephasing $\,\Delta\Phi$ as function of the initial position $p_0$. The circles display the extrapolated values when the particle arrives at the ISCO, and the curve shows a quadratic fit. In all cases the mass ratio $\eta=10^{-2}$.}
\label{fig8}
\end{figure}

After the completion of this work we became aware of Warburton {\it et al} \cite{warburton}. The approach of \cite{warburton} is similar to our osculating method, except that \cite{warburton} estimates the dephasing by the difference in the azimuthal angle $\varphi$ of the orbit, whereas we actually compute the waveforms and find their dephasing. The generalization of our quasi--circular orbit to bound orbits of varying eccentricity --- as is done in \cite{warburton} --- is straightforward, as the osculating orbits equations of motion already include the eccentricity parameter. Lastly, we compute the waveforms using two independent computational methods, specifically the osculating method and the direct method. The direct method does not appear to us to be convenient for  generalization to generic Kerr orbits, and the osculating method has a clear advantage over it for such orbits.

\section*{Acknowledgments}

The authors wish to thank Gaurav Khanna for discussions and for use of his numerical code.
This work has been supported by a NASA EPSCoR RID grant and by NSF grants PHY--0757344, PHY--1249302 and DUE--0941327. LMB is grateful to Alessandro Spallicci for hospitality.

\begin{appendix}

\section{The 5.5 Post--Newtonian term}\label{PN}

The ${\rm PN}_{5.5}$ term used in Eq.~(\ref{pn}) is given by (\cite{tanaka:1996}):

\begin{eqnarray*}
{\rm PN}_{5.5}&=& 1 - \frac{1247}{336} \Bigg(\frac{M}{r}\Bigg) + 4 \pi\Bigg(\frac{M}{r}\Bigg)^{\frac{3}{2}} -
 \frac{44711}{9072}\Bigg(\frac{M}{r}\Bigg)^2 \\
 &-& \frac{8191}{672}\ \pi \Bigg(\frac{M}{r}\Bigg)^{\frac{5}{2}}+
\Bigg( \frac{6643739519}{69854400}
 - \frac{1712}{105}\,  \gamma
+  \frac{16}{3}\  \pi^2\\
&-& \frac{3424}{105}\  \ln 2
 -\frac{856}{105} \,\ln\frac{M}{r}\Bigg)\Bigg(\frac{M}{r}\Bigg)^3
   - \frac{16285}{504} \pi \Bigg(\frac{M}{r}\Bigg)^{7/2} \\
 &+& \Bigg(-\frac{323105549467}{3178375200}+
\frac{232597}{4410}\, \gamma - \frac{1369}{126}\  \pi^2 \\
&+& \frac{39931}{294}\  \ln 2 - \frac{47385}{1568}\  \ln 3  +
  \frac{232597}{8820}\ \ln \frac{M}{r}\Bigg) \Bigg(\frac{M}{r}\Bigg)^4\\
  &+& \pi\, \Bigg(\frac{265978667519}{745113600} - \frac{6848}{105}\, \gamma
-  \frac{13696}{105}\, \ln 2 \\
&-&  \frac{3424}{105}\ \ln \frac{M}{r}\Bigg) \Bigg(\frac{M}{r}\Bigg)^{9/2}
+\ \Bigg(-\frac{2500861660823683}{2831932303200} \\
&+& \frac{916628467}{7858620}\ \gamma
- \frac{424223}{6804}\,\pi^2
- \frac{83217611}{1122660}\ \ln 2\\
&+& \frac{47385}{196}\  \ln 3
+  \frac{916628467}{15717240}\ \ln\frac{M}{r}\Bigg) \Bigg(\frac{M}{r}\Bigg)^{5} \\

&+&\pi\, \Bigg(\frac{8399309s750401}{101708006400}
+ \frac{177293}{1176}\ \gamma
+  \frac{8521283}{17640} \ \ \ln 2\\
&-& \frac{142155}{784} \ \ \ln 3
+  \frac{177293 }{2352}\  \ln\frac{M}{r}\Bigg)\Bigg(\frac{M}{r}\Bigg)^{11/2}
\end{eqnarray*}

\end{appendix}

redpajama_set_name: RedPajamaArXiv


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            handler: renderJsonHandler(articleService.toggle),
            config:{
                plugins: {'hapiAuthorization': {role: 'ADMIN'}},
                validate:{
                    params:{
                        articleId:joi.string(),
                        type:joi.boolean()
                    }
                }
            }

        });
        server.route({
            method: 'PUT',
            path: '/articles/{articleId}',
            handler: renderJsonHandler({users:articleService.save}),
            config:{
              //  auth:"simple",

                plugins: {'hapiAuthorization': {role: 'ADMIN'}},
                validate:{
                    payload:{
                        article:joi.object().required(),
                        meta:joi.object().required(),
                        _id:joi.string().optional()
                    }
                }
            }

        });
        //Images
        server.route({
           method:"POST",
            path:"/images",
            config:{
                plugins: {'hapiAuthorization': {role: 'ADMIN'}},

                payload: {
                    output: 'stream',
                    parse: true,
                    allow: 'multipart/form-data'
                }
            },
            handler:renderJsonHandler(imageService.upload)
        });
        server.route({
            method: 'GET',
            path: '/api/images',
            config:{
                plugins: {'hapiAuthorization': {role: 'ADMIN'}}
            },
            handler: renderJsonHandler({images:imageService.list})
        });
        server.route({
            method: 'GET',
            path: '/images/{p*}',
            handler: {
                directory: {
                    path:process.env.IMAGE_DIRNAME || "./tmp"
                }
            },
            config: {auth: false}
        });
        //Views
        server.route({
            method: 'GET',
            path: '/',
            handler: renderViewHandler(function () {
                return {}
            }, "index"),
           // config: {auth: "simple"}
            config: {auth: false}
        });
        server.route({
            method: 'GET',
            path: '/reset/{resetToken}',
            handler: renderViewHandler(resetPassService.getEmailByResetToken, "index"),
            //config: {auth: "simple"}
            config: {auth: false}
        });

        server.route({
            method: 'GET',
            path: '/blog',
            handler: renderViewHandler({
                user:userService.getUser,
                articles:articleService.list,
                registrationCount:userService.getRegistrationCount,
                config:configService.getConfig
            }, "index")
        });
        server.route({
            method: 'GET',
            path: '/blog/{articleId}',
            handler: renderViewHandler({article:articleService.get}, "index")
        });

        server.route({
            method: 'GET',
            path: '/admin',
            handler: renderViewHandler({users:userService.getUsers,articles:articleService.listAll,config:configService.getConfig}, "index"),
            config:{
                plugins: {'hapiAuthorization': {role: 'ADMIN'}}
            }
        });
        server.route({
            method: 'GET',
            path: '/admin/edit/{articleId}',
            handler: renderViewHandler({article:articleService.get,images:imageService.list}, "index"),
            config:{
                plugins: {'hapiAuthorization': {role: 'ADMIN'}}
            }
        });

        server.start(function () {
            console.log('Server running at:', server.info.uri);
            console.log('Server started on port: ', server.info.port);
        });

    });

redpajama_set_name: RedPajamaGithub


text:
To further clarify…
May 29th, 2011	| Filed under Uncategorized
So the Daily Mail has picked the story up.
They didn't have anything new to say, they're just basically copying what the Sunday Times said, adding the odd bit of information from my blog, but nothing significant (and certainly none of the actual points I was trying to make).. The reference to "patient zero" originating with the spread of HIV in the USA was unnecessary – it's a common phrase to mean the first person in any sort of virus – in this case, the idea of "viral information".
That said, they do have the added bonus of using a picture without permission. They can't attribute copyright to the Sunday Times, because they do not hold that copyright. Worth bothering about? Probably not..
In spite of being cheap churnalism, the Mail still manages to get some extra details wrong. For example, the Sunday Times said:
There is nothing like being told you cannot know something to pique your interest. "Curiosity got the better of me," said Webley.
'There is nothing like being told you cannot know something to pique your interest. Curiosity got the better of me,' said Webley.
Spot the difference in what part of the sentence is attributed to me, eh?
They also seem to think that I made those comments on Twitter. I'd like to see where they think I did that. If you don't know where a quote came from, don't just make something up…
And finally, the assertion that my tweet was "rapidly retweeted" – not really the case. It was retweeted twice. Twice. That's as far as it went. The original story that I took the information from got tweeted about something like thirty times. More than that, bit.ly stats on the page suggest links have been followed to it over 8,000 times from that shortening service alone. The later tweet by @theurbaninsider got hundreds of retweets, if memory serves, and attracted enough attention to be served with a take-down notice. Once again, like a broken record, I dispute my significance to the story. It's almost like the mainstream media doesn't understand how information spreads online…
Kobayashi Maru A-Level A few clarifications…
Steve Kuncewicz
May 31st, 2011 at 11:07
Looks like you may have a claim in defamation against the papers if they're wrong! May be worth letting them know.


Jennifer "J.J." Wagner Davis began her tenure as Executive Vice President and Chief Operating Officer of the University in November 2018. Along with the Executive Vice President and Provost and the Executive Vice President for Health Affairs, she serves as a member of President Ryan's executive leadership team.
In this role, Davis is the University's chief administrative, business, and operating officer and is responsible for setting financial policy and overseeing the financial affairs of the University including its schools and the Medical Center. In addition, these key operational and administrative areas report to her, in some cases through a vice president: finance, treasury, human resources, capital planning, facilities management, business operations, organizational excellence, emergency preparedness, public safety and security, information technology services, state governmental relations, and economic development. Davis serves on the boards of the University of Virginia Physicians Group, the University of Virginia Investment Management Company, and the University of Virginia Foundation.
Previously, Davis served as Senior Vice President for Administration and Finance at George Mason University for five and a half years. There she provided direction, oversight, and financial and operation management for Mason financial operations; campus police; safety, emergency & enterprise risk management; auxiliary enterprises; transportation and parking services; human resources and payroll; facilities management, planning, financing and construction; and space management.
Before moving to Virginia in 2013, Davis served the state of Delaware for almost 20 years in such capacities as Budget Director, Deputy Secretary of Education, Associate Secretary of Education for Policy and Administrative services, and as the Cabinet Secretary-Director of the Office of Management and Budget. In her last five years in Delaware, she was the Vice President for Finance and Administration at the University of Delaware, where she and her colleagues touched on nearly every aspect of the campus, from the redesign of the human resources, finance and payroll systems to revamping the compensation system.
Davis earned both her bachelor's degree in political science and her master's degree in policy analysis from Pennsylvania State University. She is married and has two children.


Buckinghamshire Mind is launching Care in Mind, a series of courses to support people with Young Onset Dementia (under the age of 65).
The courses aim to help people to continue to live well with Young Onset Dementia and to maintain wellbeing. It will be an opportunity for participants to meet others, share experiences and have fun participating in a variety of physical activities, tailored to a beginner level.
The courses are open to anyone with a Young Onset Dementia diagnosis and each participant is encouraged to bring a companion, friend or family member with them to the sessions.


1. On I-35, take exit 157, Hwy. 33.
2. Drive west on Hwy. 33, which becomes Noble Ave.
3. It is approximately 1.5 miles from I-35 to the church, which faces Noble Ave., just before you get to downtown Guthrie. The church is on the north side of Noble, which will be on your right as you proceed west.


text:
I'm going to change the subject: Shania Twain clashed with Oprah Winfrey (video)
By Frank Bojazi October 5, 2022
In an episode of Table Manners, Shania Twain describes a dream dinner she had with media mogul Oprah Winfrey, which quickly became sour when they started discussing religion. The Canadian-born singer, 57, recently recalled one of her "most memorable dinners" with the 68-year-old talk-show icon during an appearance on the "Table Manners" podcast. The podcast is hosted by Jennie and Lennie Ware.
On the podcast, Ware, 37, sparked Twain's story when she asked about a notable dinner in her life. The singer mentioned the '90s, but it's not clear when that specific dinner took place. After mentioning that she had dinner with her in a restaurant, Twain said, "She is just such a smart lady, and it's just great to sit and have real talks." "But as soon as we started talking about religion, it all went sour," she continued. "So I said, let's stop talking about religion," the "You're Still the One" Shania added, per Fox News.
According to Twain, Winfrey, 68, is "pretty religious," and she described herself as a person who is "not dedicated" to any religion. "I'm much more of a spiritual person," she stated. "I would say I'm a seeker."
Ware stated, "But at least you knew to just stop it right there." Twain agreed and said, "Right. You know how everyone always says, 'Never talk about politics or religion.'"
Winfrey and the singer of "Man! I Feel Like a Woman" seemed open to discussing religion, despite the fact that the two might disagree on it. But it wasn't long before she realized that such a conversation was impossible. The celebrity claimed, "It just wasn't debatable."
"There was no room for debate. And I like to debate. Canadians like to debate everything. So I'm like, OK, I'm going to change the subject."
Twain has made a number of appearances on Winfrey's former talk show "The Oprah Winfrey Show" through the years. Twain spoke for the first time with the host in over five years in May 2011, during which she talked about the painful breakup of her marriage with Robert "Mutt" Lange.
Winfrey attended the Baptist church and said she was a Christian. Although she prays every night, she doesn't consider herself a "traditionalist," since she doesn't attend church every Sunday, according to a 2015 interview with AARP.org.
A new '80s-inspired single called "Waking Up Dreaming" was released by Twain earlier this month. In a recent interview with The Sun, she talked about the decision to go topless for the song's cover, which also features her wearing a white shirt tied around her waist, colorful boots and a cowboy hat.
"I styled that photograph myself. It was all about taking off the bra, taking off the shirt, tying the shirt around my waist," the singer-songwriter declared to the outlet. "This is a statement of being comfortable in my own skin and just being really myself."
In addition, Twain noted that she had been diagnosed with Lyme disease and dysphonia, a condition that affected her vocal cords, resulting in a weak singing voice.
This story syndicated with licensed permission from Frank who writes about entertainment news articles. Follow Frank on Facebook


text:
Q: Oracle backup with SEQUENCE-ID Column Good morning,
I allready know how to do oracle backups with expdp and impdp. It is also no problem for me to remap backups from one schema to an other.
But know I have something where I find no solution to solve it.
I have a table with an ID column. This column has a default value based on a sequence.
 CREATE TABLE "TABLE_NAME"
   (    "ID" NUMBER(*,0) DEFAULT "TABLE_NAME_ID_SEQ"."NEXTVAL",
    "KEY" VARCHAR2(200 BYTE),
    "VALUE" CLOB
   )

After executing thise statement Oracle defines this default with "MY_USER"."TABLE_NAME_ID_SEQ"."NEXTVAL".
This is not an issue until I try to uses the backup with a different schema name. The REMAP_SCHEMA parameter of impdp seems only to change the schema definition in the tabelnames but not in the default values. So the imported backup creates a table with a default values which references to a  wrong schema.
How could I solve this?
Best regards"

redpajama_set_name: RedPajamaStackExchange


text:
Q: Denormalising a fully normalised table Can anyone advise on how to go about denormalising a fully normalised table? I've not been able to find much on it despite googling.
Whenever a record is updated (though not inserted, but lets not worry about that now) in TableA a record is inserted into HistoryOfTableA with the values of the fields which have changed and an associated timestamp when it was carried out.
eg.
TableA fields:
TableA_Id, FieldA, FieldB, FieldC, FieldD.... etc

HistoryOfTableA records:
HistID, TableA_Id, FieldChanged, OldValue, NewValue, DateCreated
1, 1, 'FieldA', 1, 2, <2013-03-18 12:20:00>
2, 1, 'FieldB', A, B, <2013-03-18 12:20:00>
3, 1, 'FieldC', A, B, <2013-03-18 12:20:00>

The situation is I'm looking to create some SQL for reporting purposes. So I want to be able to specify a point in time, and be able pull together those hostory table entries and work out what the state of that record from TableA was at that time.
I'm thinking I can create tables based on the history table and joined on the date created and the Id from table A
eg.
select HistA.NewValue,
       HistB.NewValue,
       ....
from FieldA_HistoryOfTableA HistA
     inner join FieldB_HistoryOfTableA HistB on HistA.DateCreated = HistB.DateCreated
       and HistA.TableA_Id = HistB.TableA_Id
     inner join ... etc
where HistA.FieldChanged = 'FieldA'
and HistB.FieldChanged = 'FieldB'
and .... etc...

But I don't think this is going to give me all that I want and I may not be able to do this purely in SQL. As an aside there are 20 fields in TableA so trying to join 20 tables may not be wise.

A: Your problem is not that the table is normalised, but rather that it isn't.
The data identified by fields in one table is identified by data in another table, which makes it very complicated to query.
A fully normalised version would also store the fields from TableA in a separate table:
TableA
------------
TableA_Id

TableAFields
-------------
TableA_Id
FieldId
Value

Field
---------
FieldId
FieldName

HistoryOfTableA
----------------
TableA_Id
FieldId
OldValue
ChangedDate

Now you can join in the fields from the history table. That will be a bit tricky, but at least it won't be a query with 20 joins.

A: If you want the most recent records from the history table, you can use the following SQL:
select ht.*
from (select ht.*,
             ROW_NUMBER() over (partition by FieldChanged, TableA_Id order by DateCreated desc) as seqnum
      from HistoryOfTableA ht
      where datecreated <= YOURDATEHERE
     ) ht
where seqnum = 1

If you want this as a single record, you should either pivot or do an aggregation.  Here is the latter approach:
select ht.TableA_id,
       max(case when FieldName = 'FieldA' then NewValue end) as FieldA,
       . . .
from (select ht.*,
             ROW_NUMBER() over (partition by FieldChanged, TableA_Id order by DateCreated desc) as seqnum
      from HistoryOfTableA ht
      where datecreated <= YOURDATEHERE
     ) ht
where seqnum = 1
group by TableA_id

A: You can try using a XML column in the TableA to record the history of every row in TableA. i.e. Every row has a column which is of type XML and records the history of that row. Then you can pull the rows into your application(in a batched manner if the number of rows are huge), and find out the history of each record in TableA


Ben & Jerry's CEO Jostein Solheim (left) and Friends of the Earth's biotechnology policy campaigner Eric Hoffman (right) are ice creaming against this fishy business.Photo: Friends of the Earth via FlickrMost ice cream lovers probably wouldn't line up for any flavor dubbed "Something's Fishy." That is, unless it were Ben & Jerry's phamous Phish Food in political disguise.
Because Ben & Jerry's cone not stand the thought of genetically engineered (GE) salmon — it fears GE cows will mooove in next — the company has taken an official stance against AquaBounty's GE salmon currently being examined by the FDA. Last week, the ice cream makers co-hosted a protest rally outside the White House with nonprofits Friends of the Earth, Food and Water Watch, and Center for Food Safety. In addition to heaping helpings of political activism, the company also served a "protest batch" of the cleverly re-named frozen treat, "Something's Fishy." It's "an outrageous flavor protesting genetically engineered salmon," and it's chocolatey, marshmallowy good.
Ben & Jerry's activism doesn't stop there, however. It's still very visible on the company's homepage, benjerry.com, where you can learn more about its concerns about genetically engineered food animals and play Dr. Frankenstein with the salmon swimming innocently across the page.
Even though the FDA's public commenting period has ended, I still think a special-edition Free Cone Day featuring "Something's Fishy" would really invigorate the cause. Right?


Surely, you have seen the Mountain Dew Vertical Challenge pull their flashy Dew Tour fleet up to a ski area near you. A team of energetic Dew disciples, plastered with Mountain Dew logos, set up huge inflatable soda cans, tents, and coolers full of drinks. Throughout the day, The Crew amps up the crowd with music, free soda, trivia games and a dual slalom race. The race is free, prizes are awarded at day's end, and the theme of the event is "fun". But there is more to this soft drink giveaway day than meets the eye.
"It's not just a fun race or a day of prizes at each ski resort. We are all about bringing wholesome fun to kids and their families," said Frank Tansey, of PepsiCo. Tansey has been promoting the Mountain Dew Vertical Challenge for two decades. The Dew Tour has been going for over 20 years, and thousands of free sodas. Okemo Mountain in Vermont is typically the kickoff resort for the winter tour, as has become tradition for the 30+ ski area schedule which ends at Loon in March.
You should do The Dew this year with your kids. The race is fun and free, and the benefits go beyond free soda.


The following is from a blog post by Trish Lambert on the A Pilgrim in Narnia blog.
I was asked this question not long ago. It is a good question; there is a noticeable lack of family relationships in the story. Frodo is not really Bilbo's nephew, but a cousin (and somewhat distant at that). The members of the Fellowship are all bachelors, and only two of them, Sam and Aragorn, have loved ones to unite with if their quest succeeds. Boromir, Faramir, Théodred, and Éomer—all of royal blood either in direct line to rule or one step away from direct line—are all childless bachelors in spite of being well into adulthood.
In view of all this, my simple answer is yes, I think The Lord of the Rings favors friendship, but I would not say that it is presented as "better" than familial love. I believe that Tolkien had explicit reasons for the lack of family ties that in fact ran counter to his initial inclinations.


text:
About Sargent
About Sargent Overview & History
List of Openings
Programs & Services Overview
Pediatric Program
Diagnostic & Evaluation Services
Neuro-Rehabilitation Program (Brain Injury)
Day Treatment Program
For Adolescents
Expertise in Diagnostic & Evaluation Services
Restorative Justice Practices
The Hearing Center (Audiology)
Outpatient Services & Programs
Brain Injury Continuing Ed
RRC Overview
About the RRC
RRC Programs
RRC Statewide Resource Library
RRC Login
Achieving the Extraordinary
in Rehabilitating Human Potential
Email Facebook Twitter More
About the Regional Resource Center (RRC)
In 2013, Sargent Rehabilitation Center completed the construction of the first statewide Regional Resource Center (RRC) designed to support the medical rehabilitation, education and behavioral mental health professions. The Regional Resource Center (RRC) is one of a series of program expansions at Sargent Rehabilitation Center whose history of providing quality and innovative programs for individuals with disabilities dates back nearly a century to 1917.
The RRC was built to provide education, training, technical assistance and product delivery to a variety of professional disciplines supporting education, medicine and rehabilitation. The facility is equipped with state of the art technology with ample seating capacity to accommodate moderate to large meetings and professional seminars up to 150 participants.
The RRC's unique mission is to convene knowledge. Contributions from families, education, medical and rehabilitation experts provide the leadership to advance the quality of life for individuals with disabilities of all ages and all abilities. The convening of community members supporting one another forms the basis of the Public Policy Institute existing within the RRC; ready to respond to the changing needs of society. Family focused activities are supported by our Roy T. Morgan Family Institute. Public, non-public, private and charter schools receive direct support from the RRC's Supporting Schools Project. Ongoing professional development, seminars attracting national speakers and local experts represent the RRC's commitment to ongoing education realized through our Professional Development Academy. Continuing education I supported by the RRC's University and College Affiliates. Professionals from education, medicine, rehabilitation and law converge at the RRC to exchange knowledge, share ideas and receive professional development including CEUs, CLEs, MCLEs, and PLUs (professional learning units).
The RRC is designed to serve New England with Rhode Island operating as its home.
800 Quaker Lane
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text:
Q: Sort 80,412 files into folders based on name begins with Situation:

*

*a folder with 80,412 files

*all files named with CamelCase, some have a dash (-) separating the first word

*files can be grouped by beginning with the same word or letters(i.e. "ClientslistRebecca..." and "Clientslist-Adam...")

*no file name begins with a number

*very few files begin with a unique word

I need to take the first word, find all files that begin with that word, and create a folder named with that word. Repeat for all files.
The main complication is that sometimes a name begins with multiple capitals, followed by a word that also begins with a capital (i.e. "AWDRebecca..."). Not sure how to resolve that, but I'm fine with doing some manual cleanup afterwards if I get folders with "AWDRebecca", "AWDReports", "AWDNovember", but having a folder "A" will make it harder.

A: A shell snippet like
for i in *; do
  case "$i" in
    [A-Z][A-Z]*) # $i has several leading caps
        dir=$(sed -E -e 's|([A-Z]+)[A-Z].*|\1|' <<< "$i")
        echo mkdir -p "$dir"
        echo mv "$i" "$dir"/
        ;;
    [A-Z][a-z]*) # $i has one leading cap
        dir=$(sed -E -e 's|([A-Z][a-z]+).*|\1|' <<< "$i")
        echo mkdir -p "$dir"
        echo mv "$i" "$dir"/
        ;;
    *) echo "Huh: $i"
       ;;
  esac
done

should work. As written it will just print the commands on the screen. If they look sensible, remove the four echo before mkdir/mv.
Also, for 80'000 files, the for i in * part may fail. If this is the case, run it in batches with for i in [A-E]*, for i in [F-K]* etc.
PS: It will fail for files with a ALLCAPS name. If you have does, please comment so I can add another rule.


text:
Q: Powershell SelectSingleNode on a child node I'm using Powershell to install an SSIS Project and create a Environment for it.  I am reading the project parameters from the Project.Params XML file to create the environment variables & their values.  I am able to use the following code snippet to read the parameters & their values, but I'd like to use SelectSingleNode instead of the second foreach loop. My XPath skills are not up to it.
Here's the working code:
# load the Params file into memory
[xml]$ParamsDoc = Get-Content -Path $ParamsFilePath

# for each parameter in the Params file, add an environment variable if it doesn't already exist
foreach ($Param in $ParamsDoc.Parameters.Parameter)
{
    $ParamName = $Param.Name

    # use the value in the Params file as the default value for the environment variable
    foreach ($Prop in $Param.Properties.Property)
    {
        if ($Prop.Name -eq 'value')
        {
            $ParamValue = $Prop.InnerText
            break
        }
    }
    AddEnvironmentVariableIfMissing $ParamName $ParamValue
}

AddEnvironmentVariableIfMissing is a separate function I've written.  Now, here's the code that doesn't work:
# load the Params file into memory
[xml]$ParamsDoc = Get-Content $ParamsFilePath

$nsMgr = New-Object System.Xml.XmlNamespaceManager($ParamsDoc.NameTable)
$nsMgr.AddNamespace("SSIS", $ParamsDoc.DocumentElement.NamespaceURI)

foreach ($Param in $ParamsDoc.Parameters.Parameter)
{
    $ParamName = $Param.Name

    # NONE of these work!
    $ParamValue = $Param.Properties.SelectSingleNode("SSIS:Property[@Name='Value']",$nsMgr)
    $ParamValue = $Param.Properties.SelectSingleNode("Name[.='Value']",$nsMgr)
    $ParamValue = $Param.Properties.SelectSingleNode("SSIS:Property/Name[.='Value']",$nsMgr)
    $ParamValue = $Param.Properties.Property.SelectSingleNode("Name[.='Value']",$nsMgr)
    $ParamValue = $Param.SelectSingleNode("SSIS:Properties/SSIS:Property[@Name='Value']",$nsMgr)
    $ParamValue = $Param.SelectSingleNode("SSIS:Properties/SSIS:Property/Name[.='Value']",$nsMgr)
    $ParamValue = $Param.SelectSingleNode("SSIS:Property[@Name='Value']",$nsMgr)
    $ParamValue = $Param.SelectSingleNode("SSIS:Property/Name[.='Value']",$nsMgr)

    AddEnvironmentVariableIfMissing $ParamName $ParamValue
}

What is the correct XPath syntax to get the child node with Name = 'Value'?
Here's a sample of an SSIS Project.params file
<?xml version="1.0"?>
<SSIS:Parameters xmlns:SSIS="www.microsoft.com/SqlServer/SSIS">
  <SSIS:Parameter
    SSIS:Name="Client">
    <SSIS:Properties>
      <SSIS:Property
        SSIS:Name="ID">{144b0266-9e94-4821-bb68-f020436d5df5}</SSIS:Property>
      <SSIS:Property
        SSIS:Name="CreationName"></SSIS:Property>
      <SSIS:Property
        SSIS:Name="Description"></SSIS:Property>
      <SSIS:Property
        SSIS:Name="IncludeInDebugDump">0</SSIS:Property>
      <SSIS:Property
        SSIS:Name="Required">0</SSIS:Property>
      <SSIS:Property
        SSIS:Name="Sensitive">0</SSIS:Property>
      <SSIS:Property
        SSIS:Name="Value">sampleclient</SSIS:Property>
      <SSIS:Property
        SSIS:Name="DataType">18</SSIS:Property>
    </SSIS:Properties>
  </SSIS:Parameter>
  <SSIS:Parameter
    SSIS:Name="MSSQLServer">
    <SSIS:Properties>
      <SSIS:Property
        SSIS:Name="ID">{b4e6c5e1-ef85-4df3-b2dc-db37971d081d}</SSIS:Property>
      <SSIS:Property
        SSIS:Name="CreationName"></SSIS:Property>
      <SSIS:Property
        SSIS:Name="Description"></SSIS:Property>
      <SSIS:Property
        SSIS:Name="IncludeInDebugDump">0</SSIS:Property>
      <SSIS:Property
        SSIS:Name="Required">0</SSIS:Property>
      <SSIS:Property
        SSIS:Name="Sensitive">0</SSIS:Property>
      <SSIS:Property
        SSIS:Name="Value">MSSQLSERVER</SSIS:Property>
      <SSIS:Property
        SSIS:Name="DataType">18</SSIS:Property>
    </SSIS:Properties>
  </SSIS:Parameter>
</SSIS:Parameters>

A: So PetSerAI had the right idea. The namespace needed to be in the XPath syntax, including the Name element.  The two syntax that work are:
    $ParamValue = $Param.Properties.SelectSingleNode("SSIS:Property[@SSIS:Name='Value']",$nsMgr)
    $ParamValue = $Param.SelectSingleNode("SSIS:Properties/SSIS:Property[@SSIS:Name='Value']",$nsMgr)

Thank you, PetSerAI !


Google Plus has finally decided to ban all the users using pseudonyms and nicknames in place of their real names. Though users will not be suspended immediately for violating Google Plus Common Names Policy, they will be given four day grace period to fix their profile names before they're suspended.
Google Plus Common Names Policy is designed to fight spam and prevent the creation of fake profiles. The suspension of users using pseudonyms or nicknames has resulted in criticism among various users. Though this criticism hasn't stopped Google Plus from deciding to eliminate the use of pseudonyms on its social network.
A quick tip - all users should update their profile as soon as possible to prevent their Google Plus profile from being suspended.
thats definitely not a good step by google plus, this is drive some people away,but what then there's always a way out and developers won't admit it though.thats definitely not a good step by google plus, this is drive some people away,but what then there's always a way out and developers won't admit it though.
no google is making a right move. i'm fedup of users using nicknames, it hard to recognize at times.


text:
Q: Beta constraints in H2OGeneralizedLinearEstimator I'm looking for a way to set beta in prior to the model run in H2O GeneralizedLinearEstimator? Beta which can be used as a starting point for the model? It is called beta constraints as per the documentation below. Could someone help me with this.
http://docs.h2o.ai/h2o/latest-stable/h2o-docs/data-science/algo-params/beta_constraints.html
Here is the example what I'm trying
1)   Model 1: I ran a model with 20 iterations and used the betas from this model run and saved it as a data frame
2)   Model 2: I ran a model with everything the same as the first Model (including 20 iterations), additionally I specified beta constraints as the coefficient from the previous model. Trying to warm start this model so it starts where the previous model ended.
3)   Model 3: I ran a model with everything the same as the first model but with 40 iteration
As explained in the documentation I wanted to compare and see that the model 2 betas to be same as the betas from a model 3
Code with beta constraints specification
    model2 =  H2OGeneralizedLinearEstimator(family = "poisson",
                                            alpha=0,
                                            solver = "L-BFGS",
                                            max_iterations=20,
                                            gradient_epsilon=1e-8,
                                            objective_epsilon=1e-8,
                                            beta_epsilon=1e-8,
                                            beta_constraints=bc)

A: According to the H2O Glossary, the format for beta_constraints is:

A data.frame or H2OParsedData object with the columns ["names",
  "lower_bounds","upper_bounds", "beta_given"], where each row
  corresponds to a predictor in the GLM. "names" contains the predictor
  names, "lower_bounds" and "upper_bounds" are the lower and upper
  bounds of beta, and "beta_given" is some supplied starting values for
  beta.

First, you need to get the vector of betas from Model 2. Call them m2_betas.
Next, because you want strict equality constraints, you need to and set those to the upper bounds, lower bounds, and starting value.
I have done this in R (see related answer), where beta_constraints are passed as a data.frame but I assume that the Python API is similar and uses a pandas.DataFrame. Try:
constraints = pd.DataFrame({'names':x.columns,
                             'lower_bounds':m2_betas,
                             'upper_bounds':m2_betas,
                             'beta_given':m2_betas})


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