text:
Q: How to extend control templates (for example with a third color) I do have a control template for WPF button. Within the template I can use the Fillcolor and Backcolor of the button. But is it possible to define a third color that can be used in the template and later on in a real button?
Here an example of a circular button. I would like to add a color for the ToggleButton.IsChecked state.
<ControlTemplate x:Key="MyButtonTemplate" TargetType="{x:Type ToggleButton}">
    <Grid>
        <Ellipse x:Name="outerCircle" Width="Auto" Height="Auto" StrokeThickness="4" Fill="White" Stroke="Gray"/>
        <Label x:Name="content" Content="{TemplateBinding Content}" HorizontalAlignment="Center" VerticalAlignment="Center" Foreground="Gray"/>
    </Grid>
    <ControlTemplate.Triggers>
        <Trigger Property="IsChecked" Value="True">
            <Setter TargetName="outerCircle" Property="Fill" Value="{Binding Path=Foreground, RelativeSource='{RelativeSource TemplatedParent}'}"/>
        </Trigger>
        <Trigger Property="IsEnabled" Value="False">
            <Setter TargetName="outerCircle" Property="Fill" Value="LightGray"/>
        </Trigger>
        <Trigger Property="IsMouseOver" Value="True">
            <Setter TargetName="outerCircle" Property="Fill" Value="{Binding Path=Foreground, RelativeSource='{RelativeSource TemplatedParent}'}"/>
            <Setter TargetName="content" Property="Foreground" Value="Gray"/>
        </Trigger>
    </ControlTemplate.Triggers>
</ControlTemplate>

A: I am not sure wether or not you want to bind this to a property or just use a brush resource, Here is an example using a Resource:
<Window x:Class="WpfApplication1.MainWindow"
    xmlns="http://schemas.microsoft.com/winfx/2006/xaml/presentation"
    xmlns:x="http://schemas.microsoft.com/winfx/2006/xaml"
    Title="MainWindow" Height="350" Width="525">
    <Window.Resources>
        <SolidColorBrush x:Key="ControlPressedColor">#FF211AA9</SolidColorBrush >
        <ControlTemplate x:Key="MyButtonTemplate" TargetType="{x:Type ToggleButton}">
            <Grid>
                <Ellipse x:Name="outerCircle" Width="Auto" Height="Auto" StrokeThickness="4" Fill="White" Stroke="Gray"/>
                <Label x:Name="content" Content="{TemplateBinding Content}" HorizontalAlignment="Center" VerticalAlignment="Center" Foreground="Gray"/>
            </Grid>
            <ControlTemplate.Triggers>
                <Trigger Property="IsChecked" Value="True">
                    <Setter TargetName="outerCircle" Property="Fill" Value="{StaticResource ControlPressedColor}"/>
                </Trigger>
                <Trigger Property="IsEnabled" Value="False">
                    <Setter TargetName="outerCircle" Property="Fill" Value="LightGray"/>
                </Trigger>
                <Trigger Property="IsMouseOver" Value="True">
                    <Setter TargetName="outerCircle" Property="Fill" Value="{Binding Path=Foreground, RelativeSource='{RelativeSource TemplatedParent}'}"/>
                    <Setter TargetName="content" Property="Foreground" Value="Gray"/>
                </Trigger>
            </ControlTemplate.Triggers>
        </ControlTemplate>
    </Window.Resources>
    <Grid>
        <ToggleButton Template="{StaticResource MyButtonTemplate}"  Height="50" Width="50"></ToggleButton>
    </Grid>
</Window>

Base on the clarification that you wanted to be able to set the property on the ToggleButton you will need to use a Dependecy Property here is a quick example:
Custom Control
using System;
using System.Collections.Generic;
using System.Linq;
using System.Text;
using System.Windows;
using System.Windows.Controls;
using System.Windows.Data;
using System.Windows.Documents;
using System.Windows.Input;
using System.Windows.Media;
using System.Windows.Media.Imaging;
using System.Windows.Navigation;
using System.Windows.Shapes;

namespace WpfApplication1
{

    public class CustomControl2 : System.Windows.Controls.Primitives.ToggleButton
    {
        public static readonly DependencyProperty myFillColorProperty = DependencyProperty.Register("myFillColor",typeof(SolidColorBrush),typeof(System.Windows.Controls.Primitives.ToggleButton));
        static CustomControl2()
        {
            DefaultStyleKeyProperty.OverrideMetadata(typeof(CustomControl2), new FrameworkPropertyMetadata(typeof(CustomControl2)));
        }

        public SolidColorBrush myFillColor
        {
            get { return (SolidColorBrush)GetValue(myFillColorProperty); }
            set { SetValue(myFillColorProperty, value); }

        }
    }
}

MainWindow.xaml
<Window x:Class="WpfApplication1.MainWindow"
    xmlns="http://schemas.microsoft.com/winfx/2006/xaml/presentation"
    xmlns:x="http://schemas.microsoft.com/winfx/2006/xaml"
    xmlns:my ="clr-namespace:WpfApplication1"
    Title="MainWindow" Height="350" Width="525">
    <Window.Resources>
        <ControlTemplate x:Key="MyButtonTemplate" TargetType="{x:Type ToggleButton}">
            <Grid>
                <Ellipse x:Name="outerCircle" Width="Auto" Height="Auto" StrokeThickness="4" Fill="White" Stroke="Gray"/>
                <Label x:Name="content" Content="{TemplateBinding Content}" HorizontalAlignment="Center" VerticalAlignment="Center" Foreground="Gray"/>
            </Grid>
            <ControlTemplate.Triggers>
                <Trigger Property="IsChecked" Value="True">
                    <Setter TargetName="outerCircle" Property="Fill" Value="{Binding Path=myFillColor, RelativeSource='{RelativeSource TemplatedParent}'}"/>
                </Trigger>
                <Trigger Property="IsEnabled" Value="False">
                    <Setter TargetName="outerCircle" Property="Fill" Value="LightGray"/>
                </Trigger>
                <Trigger Property="IsMouseOver" Value="True">
                    <Setter TargetName="outerCircle" Property="Fill" Value="{Binding Path=Foreground, RelativeSource='{RelativeSource TemplatedParent}'}"/>
                    <Setter TargetName="content" Property="Foreground" Value="Gray"/>
                </Trigger>
            </ControlTemplate.Triggers>
        </ControlTemplate>
    </Window.Resources>
    <Grid>
        <my:CustomControl2 myFillColor="Red" Template="{StaticResource MyButtonTemplate}"  Height="50" Width="50"></my:CustomControl2>
    </Grid>
</Window>

A: You could add your ColorBrush to a ResourceDictionary, give it a key via the x:Key property and reference that resource via the StaticResource or DynamicResource markup extension from both the template and the "real" button (by which I assume you mean an instance of Button, probably defined in xaml). This requires that you merge in the dictionary that contains that key via the ResourceDictionary.MergedDictionaries property.
<Window x:Class="WpfApplication3.MainWindow"
    xmlns="http://schemas.microsoft.com/winfx/2006/xaml/presentation"
    xmlns:x="http://schemas.microsoft.com/winfx/2006/xaml"
    Title="MainWindow" Height="350" Width="525">
<Window.Resources>
    <SolidColorBrush x:Key="MySharedColor"  Color="Red"/>
    <ControlTemplate x:Key="MyTemplate"  TargetType="{x:Type Button}">
        <Border Background="{StaticResource MySharedColor}"/>
    </ControlTemplate>
</Window.Resources>
<Grid>
    <Button Style="{StaticResource MyTemplate}" BorderBrush="{StaticResource MySharedColor}"/>
</Grid>

redpajama_set_name: RedPajamaStackExchange


text:
The 1988 UC Davis football team represented the University of California, Davis as a member of the Northern California Athletic Conference (NCAC) during the 1988 NCAA Division II football season. Led by Jim Sochor in his 19th and final season, UC Davis compiled an overall record of 7–3–1 with a mark of 5–0 in conference play, winning the NCAC for the 18th title consecutive season. 1988 was the team's 19th consecutive winning season. With the 5–0 conference record, the team stretched their conference winning streak to 41 games dating back to the 1981 season. The Aggies were ranked No. 13 in the final NCAA Division II poll. They advanced to the NCAA Division II Football Championship playoffs, where they lost to Sacramento State in the first round. The team outscored its opponents 300 to 180 for the season. The Aggies played home games at Toomey Field in Davis, California.

Sochor's career at UC Davis was remarkable in its success. His teams won the conference championship in 18 of his 19 years, including 18 straight from 1971 to 1988, and reached the postseason in nine seasons. His teams had a winning record in all 19 seasons, compiling an overall record of 156–41–5, for a .785 winning percentage. In conference play under Sochor, UC Davis was 92–6, for a .939 winning percentage. Sochor was inducted into the College Football Hall of Fame in 1999.

Schedule

References

UC Davis
UC Davis Aggies football seasons
Northern California Athletic Conference football champion seasons
UC Davis Aggies football

redpajama_set_name: RedPajamaWikipedia


text:
SciArtFriday: Movie Madness
Welcome to SciArt-Fridays: A Curated List of SciArt events for the Artful Explorer.
As the clock finally strikes 5:00, and you speed through the crowds to meet friends for much needed R&R, skip the happy hour for an event a bit more experimental. In this hot hot heat, what better way to spend your nights than chilling with friends at the theater. This week, SciFriday is bringing some seriously fun, and some all-around funky films for your viewing pleasure.
SciArt Center is showing 2 Screenings in 2 Weeks, talk about the power of film
The Lower East Side, a great neighborhood for an afternoon art stroll on a sunny afternoon, or an art-filled night on the town. Skip your usual peruse of the open-air Asian markets this time to join SciArt enthusiasts at the SciArt Center. From a pop-culture blockbuster to a local documentary, the Center is hosting a few movie-packed nights that will fit into anyone's weekly culture roundabout.
By Danielle Kalamaras
"I'm sorry, Dave. I'm afraid I can't do that." - Hal
Tuesday, 7/1: SciArt Mixer Night with 2001: A Space Odyssey film screening, 7-9p.m.
SciArt Center is launching a monthly mixer, and to kick this event off the center will be screening a fan favorite Kubrick film. Sip on wine and chat with the great pool of artists, scientists, and all those in between at this great event that is free to the public.
Wednesday, 7/9: Noah Hutton Film Screening, 8-10:30p.m.
Filmmaker Noah Hutton will be presenting his work in progress documentary, Bluebrain, which follows the worldwide quest to map the human brain.
SciArt Center
21 Ludlow
Tuesday-Sunday: 12-6:30p.m.
info@sciartcenter.org
www.sciartcenter.org
Nitehawk's SciFi phase is happening this week, and that's a great thing
This movie-house gem in Williamsburg is the perfect dinner-and-a-movie at one location. With table service and a great menu of meals and trendy snacks—not to mention the full bar and crafty cocktail menu—you realize nothing beats good eats and a great movie on the big screen.
Alejandro Jodorowsky's Holy Mountain with live-music Friday, 07/01 at Midnight
Jodorowsky is a mastermind, an auteur extraordinaire, and one of the most eccentric visionaries of the 20th century. Embodying the sex, drugs, spiritual awakenings and societal unrest of the late 1960s, Jodorowsky's Mexican-American film Holy Mountain (La Montaña Sagrada) is a suitably bizarre and exquisitely designed trip. Part of NiteHawk's Summer of Surrealism series, LIVE SOUND CINEMA presents Alejandro Jodorowsky's Holy Mountain with a live score by REEL ORCHESTRETTE.
"I belong to the front. You belong to the tail." - Mason
Bong Joon Ho's Snowpiercer, opening Friday, 06/27
A perfect pairing of SciFi/Horror, this saga is a dystopian tale of class conflict. After the Earth freezes over, the few remaining humans live on the Snowpiercer, a train on an infinite loop around the globe. For those at the front, it's a lavish paradise of drugs and sushi in the lap of luxury; for those trapped in the tail section, life is short and cruel. But change is in the air. If you like metaphysical battles of ethical humanity, and great fighting scenes with supurb cinematography, this film is a must see.
Nitehawk Cinema
136 Metropolitan Ave., Williamsburg
info@nitehawkcinema.com
www.nitehawkcinema.com
IFC Center is screening Roman Polanski's surreal Venus in Fur through Tuesday, 07/01
Surrealism is running strong this summer—the mixture of esoteric and uncanny transforms any bland afternoon into a deviant adventure. Polanski is a masterful director whose movies explore the often frightening boundaries of an individual's mind. Adapted from David Ives's Broadway hit, Venus in Fur stars Thomas, a stage director auditioning a new female lead: a woman who takes a man as her slave. But when the volatile and erotic Vanda comes barreling into his Paris theater, she stuns Thomas with her commitment to the role, and the boundaries between life and art begin to crumble.
323 Sixth Avenue at W. Third St., East Village
www.ifccenter.com
BAM bringing Ridley Scott's Alien back to the big-screen Thursday, 07/3 at 7:30p.m.
BAM's #ThrowBackThursday this week is a classic film us millennials missed the chance to see in theaters when it debuted in 1979. Thankfully NYC is all about reprising cult classics. Pitting one of the great sci-fi heroines against some of the most terrifying movie creatures of all time, this brilliantly paced classic follows a space crew as they respond to a distress signal from an unexplored planet. Ridley Scott slowly creates an atmosphere of dread and escalating terror, one that continues to influence contemporary horror film-making.
BAMcinématek
Peter Jay Sharp Building
30 Lafayette Ave.
www.bam.org

redpajama_set_name: RedPajamaCommonCrawl


text:
\section{Introduction}

The discovery of gravitational waves (GW) has given us the new probe for observing the universe~\cite{PhysRevLett.116.061102}.
The typical strain sensitivity, $h$, of second generation interferometric detectors, such as Advanced LIGO~\cite{0264-9381-32-7-074001}, Advanced Virgo~\cite{0264-9381-32-2-024001}, and KAGRA~\cite{0264-9381-29-12-124007, PhysRevD.88.043007}, is around $10^{-23}/\sqrt{\mathrm{Hz}}$ at 100 Hz.

In GW150914 event data analysis, it has been shown that the calibration errors give significant impact on the sky localization accuracy.
The 90~\% sky confidence region gets larger from $150~\mathrm{deg}^2$ to $610~\mathrm{deg}^2$ by introducing the calibration uncertainties of 10~\% in amplitude and 10 degrees phase~\cite{PhysRevD.93.122004}, and eventually got smaller to $230~\mathrm{deg}^2$ with the improved calibration uncertainties~\cite{PhysRevX.6.041015, PhysRevD.96.102001}.
Using GW signals from compact binary coalescences events, researchers can derive several parameters of the source objects such as masses, spins, luminosity distance, orbital inclination and the sky location.
The precision of these derived parameters is potentially limited by the calibration accuracy. As the number of detected sources increases and events with higher signal-to-noise ratio (SNR) are detected, calibration uncertainty
will become the dominant source of errors when extracting physical informations from the signals.
Testing general relativity has been demonstrated with the GW events from binary black hole mergers~\cite{PhysRevLett.116.221101}. In most of the analysis, the effect of calibration uncertainties on the detection and parameter estimation of GW events have focused on placing constrains on the calibration accuracy by modeling the calibration errors as smooth and random frequency-dependent fluctuations. By a semi-analytic approach to explicitly relate systematic errors in calibration parameters to the GW signal parameters, it has been shown that for events with SNR$\sim20$, calibration accuracy of a few percent is required for certain parameters such as optical gain and actuation strength in order to achieve noise-limited systematics~\cite{Hall:2017off}.
Upper limits and observations of continuous GW waves such as rapidly rotating neutron stars and stochastic background of unresolvable sources depend on calibration uncertainties. The associated uncertainties on the upper limits of continuous waves amount to $\sim20~\%$ by including 10~\% amplitude calibration uncertainty~\cite{0004-637X-839-1-12,PhysRevD.96.122004}.
The suppression of the calibration error also improve burst GW reconstruction.
Especially, the precise correction of the frequency dependence will remove the
biases on arrival time and polarization components. These parameters affects on
estimations for a source direction and rotational axis of Super Novae core, respectively.
In the idea to estimate a mass of an isolated neutron star using gravitational waves~\cite{PhysRevD.91.084032,1742-6596-716-1-012026}, it must determine the phase difference precisely between once and twice spin frequency modes. For many known pulsar cases, these frequencies are around the unity gain frequency where the transfer function phase changes steeply. Also, since the continuous wave measurement would use a long-duration data sets as a order of years, the robustness and stableness of calibrations is essentially important.
In particular, the uncertainty in the absolute amplitude of the GW signal
propagates directly into the estimation of the distance to the sources.
The rate that compact binary system coalescences in the universe if drawn from detected events. The SNR by the searches are quadratically sensitive to the calibration errors since they are maximized over arrival time, waveform phase, and the template banks. The amplitude calibration uncertainty of 10~\% and the derived uncertainty of the luminosity distances of the sources corresponds to an approximately 30~\% uncertainty in volume and will dominate over the statistical uncertainty~\cite{2041-8205-833-1-L1}.
The detection of a GW signal from the GW170817 Binary Neutron Star (BNS) system, along with a concurrent electromagnetic (EM) signal, began a new era of multi-messenger astronomy~\cite{PhysRevLett.119.161101}. These observations
allow us to use GW170817 as a standard
siren~\cite{Abbott:2017xzu,Schutz_1986,Holz_2005,Nissanke_2010} with witch we can
determine the absolute luminosity distance to the source directly from the
GW signals. Assuming an event rate of 3000 Gpc$^{-3}$yr$^{-1}$
which is consistent with the 90~\%
confidence interval for GW170817~\cite{PhysRevLett.119.161101},
we expect that GW signals will be detected from about
50 BNS standard sirens dureing the next few observing runs.
These observations can constrain the Hubble constant ($H_0$) to 2~\% error or less~\cite{Feeney:2018mkj}, and eventually resolve
the 3-$\sigma$ tension in $H_0$ measurements between Cephied-SN distance
ladder~\cite{Riess_2016} and CMB data when assuming the $\Lambda$CDM
model.~\cite{2016-planck} Systematic errors in the calibration of
the absolute GW signal amplitude must be suppressed less than 1~\% to
achieve higher-precision $H_0$ measurements using GW standard sirens.

Laser interferometers measure change in distance along the two interferometer arms. Fluctuations in the degree of freedom of the differential arm length (DARM) are suppressed by a DARM control loop. The reconstruction of the DARM fluctuation at the observation frequency is affected by the GWs. The gravitational waveform can be reconstructed from the calibrated error and control signals of this DARM loop. To calibrate these signals, accurate physical models of the actuator and sensing function are essential. These models require measurements of the transfer function and monitoring of the time dependency of the transfer function using continuous sine waves (calibration lines). The residual of the time-dependent model corresponds to the uncertainty of the observaton.

To reduce the systematic uncertainty in the calibration, we need to inject well-parameterized calibration lines for the photon calibrator (Pcal) or other calibration sources for monitoring the time variation of the interferometer responce. The Pcal was developed by the Glasgow and GEO600 reserch groups~\cite{CLUBLEY200185,MOSSAVI20061}, followed by Advanced LIGO which particularly improved Pcals for calibrating the time-dependent response of interferometers~\cite{0264-9381-32-2-024001, doi:10.1063/1.4967303,0264-9381-27-8-084024,0264-9381-26-24-245011,0264-9381-32-2-024001}. However, Pcal still face a challenges in finding of the absolute amplitude calibration because of the uncertainty in the laser power standards published by different national metrology institutes~\cite{EUROMET}. The absolute power between these institutes vary by a few \% \footnote{Figure. 9 at page 46. from \cite{EUROMET} shows the absolute power measurement between the standard institute from nine countries. The systematic discrepancies between nine countries are as large as 3.5 \%.}.

Gravity field calibrator (Gcal) is one of the most promising candidates to be able to solve the uncertainty problem of the absolute laser amplitude calibrations. The technology has been developed and tested by Forward and Miller~\cite{doi:10.1063/1.1709366}, Weber~\cite{PhysRevLett.18.795,PhysRev.167.1145}, University of Tokyo~\cite{Hirakawa,1347-4065-19-3-L123,1347-4065-20-7-L498,PhysRevD.26.729,PhysRevD.32.342} and Rome university group~\cite{Astone1991, Astone1998}. Related techniques using Gcal are discussed in Matone {\it et. al.} and Raffai {\it et. al.}~\cite{0264-9381-24-9-005, PhysRevD.84.082002}. The device can modulate a test mass using a gravity gradient generated by a rotor that depending on the masses, distance, frequency, radius, and the gravity constant.

This paper proposes new method for achieving sub-percent uncertainty in the absolute amplitude calibration of the GW detectors. The method combines Pcal and Gcal.
Section~\ref{sec:Pcal} explains the methods used for Pcal. In section~\ref{sec:Gcal}, we discuss the principle of a multipole moment of gravity and how it is modulated to derive a calibration signal.
We demonstrate how to calibrate absolute displacement using two calibrators in concert in section \ref{sec:PGCAL}, and in section~\ref{sec:EST}, we discuss the contributions of the systematic error and estimate the current technological limits on the gravitational wave observation from typical physical assumptions.

\section{Photon calibrator} \label{sec:Pcal}
Pcal exploit how the photon radiation pressure from power-modulated laser beams reflects from a test mass. The periodic photon recoil applies a periodic force to test mass~\cite{doi:10.1063/1.4967303}.
Advanced LIGO, Advanced Virgo and KAGRA employ Pcals for the calibration of the interferometer response~\cite{0264-9381-34-1-015002, KAGRA_Pcal,0264-9381-32-2-024001}. All of them use laser of the same wave length, 1047~nm, to actuate the test mass. The test mass displacement is described as
\begin{equation}
 x = \frac{2P \cos{\theta}}{c} s(\omega)\left(1+\frac{M}{I}\vec{a} \cdot \vec{b} \right) , \label{eq:pcal}
\end{equation}
where $P$ is the absolute laser power, $\theta$ is the incident angle of the Pcal laser, $M$ is the mass of test mass, $\omega$ is the angular frequency of the laser power modulation, and $\vec{a}$ and $\vec{b}$ are the position vectors of the Pcal laser beams. A schematic view of device is shown in Fig.~\ref{fig:Pcal}. $I=Mh^2/12+Mr^2/4$ is the moment of inertia, where $h$ and  $r$ are the thickness and radius of the test mass, respectively. $s(\omega)$ is the transfer function between force and displacement. We can regard the value of $s(\omega)$ as $1/(M \omega^2)$ at the frequency above 20 Hz, as the test mass behaves as a free mass in this regime.

The amplitude of the laser power noise is stabilized to be less than the design sensitivity. As shown in Fig.~\ref{fig:Pcal}, the power stabilized laser is mounted on the transmitter module. The power of the photo detector responses at the transmitter module, $V_{\mathrm{TxPD}}$, and receiver module, $V_{\mathrm{RxPD}}$ are monitored for differences.
The largest relative
uncertainty of photon calibrator is that of laser power.
Advanced LIGO and KAGRA use a working standard to cross-calibrate the relative interferometer responces. The relative uncertainty of each calibrator is 0.51 \%~\cite{doi:10.1063/1.4967303}.
The second largest relative uncertainty is the optical efficiency of the optical path in the calibrator. We calibrate the injected power from the exterior of the vacuum chamber. Therefore, we need to consider the difference in optical efficiency due to the transmittance of the vacuum window and the reflectance of the mirrors. The measured uncertainty of the optical efficiency in the Advanced LIGO is 0.37 \%.
For absolute calibration, the photo detector, following the so called gold standard, is calibrated using the laser power standard maintained by the National Institute of Standards and Technology (NIST) in Boulder, CO~\cite{taylor:1994:GEEU} in the U.S.
The working standard responces for Hanford, Livingston and KAGRA GW detectors are calibrated to this gold standard.
However, a comparison of the accuracies of the absolute laser power standards maintained by each national standard institute shows a few~\%
uncertainty~\cite{EUROMET}.
 This uncertainty leads to the serious systematic error in the distance calibrations propagated from the uncertainty of the absolute calibration.

\begin{figure}
\begin{center}
\includegraphics[width=12cm]{Pcal.eps}
\caption{Schematic view of photon calibrator. The stabilized laser is placed on the transmitter module. The signal injected to the test mass is monitored through the difference in photo detector responce power between the transmitter module and  receiver module,$V_{TxPD}$  and $V_{RxPD}$. The geometrical factor is characterized in term of the position vectors of the photon calibrator beams, $\vec{a}=\vec{a_1}+\vec{a_2}$, and the main beam, $\vec{b}$.}
\label{fig:Pcal}
\end{center}
\end{figure}

\begin{table}
\begin{center}
\caption{Specification summary of Advanced LIGO, Advanced Virgo and KAGRA photon calibrator. \label{pcal}}
\footnotesize
\begin{tabular}{cccc}
\hline
& KAGRA& Advanced LIGO& Advanced Virgo \\
\hline
Mirror material & Sapphire & Silica & Silica \\
 Mirror mass & 23 kg & 40 kg & 40 kg \\
  Mirror diameter & 220 mm & 340 mm & 350 mm \\
    Mirror thickness & 150 mm & 200 mm & 200 mm \\
 Distance from Pcal & 36 m & 8 m & 1.5 m \\
to test mass &&& \\
  Pcal laser power & 20 W & 2~W & 3 W \\
  Pcal laser frequency & 1047 nm & 1047 nm &1047 nm\\
  Incident angle& 0.72 deg & 8.75 deg &30 deg \\
  \hline
\end{tabular}
\end{center}
\end{table}

\section{Gravity field calibrator} \label{sec:Gcal}
To address  this problem of uncertainty in the the absolute calibration, we propose a new calibration method that combines Pcal and Gcal.
 The Gcal generates a dynamic gravity field  by rotating the multipole masses with a rotor placed in a vacuum chamber that isolates acoustic noise. To monitor the frequency of this rotation, an encoder with
a 16-bit analog to digital converter is included.
Next, we calculate the displacement of the test mass in the dynamic gravity field generated by a multipole moment with N masses.
The calculation assumes a free-mass of a test mass and a set of masses mounted on a disk as shown in Fig ~\ref{fig:dim}.
The rotating the masses $m$ are arranged around the rotor at radius, $r$.
The distance between the center of this rotor and the test mass mirror is assumed $d$.
We rotate the disk rotates at the angular frequency $\omega_{\mathrm{rot}}=2\pi f_{\mathrm{rot}}$.

\begin{figure}
\begin{center}
\includegraphics[width=12cm]{dim.eps}
\caption{Schematic of Gcal. The rotor is placed at  the same height as the test mass and at a distance of $d$. Multipole masses spinning around the rotor generate a varying gravitational potential at the position of test mass.}
\label{fig:dim}
\end{center}
\end{figure}
We estimate the equation of motion of the test mass as it is moved by the dynamic gravity field.
First, we calculate the distance between the test mass and the N pieces of masses arranged around the rotor.
The distance between i-th mass and the center of test mass is written as
\begin{equation}
L_i=d \sqrt{1+\left( \frac{r}{d} \right)^2 -2\left( \frac{r}{d} \right) \cos{\phi_i} },
\end{equation}
where the angle of the i-th mass is assumed to be $\phi_i=\omega_{\mathrm{rot}} t + 2\pi i/N$.
The gravitational potential at the center of test mass can be described as
\begin{eqnarray}
V &=& \Sigma^N_{i=0} V_i, \\
&=& -GMm \Sigma^N_{i=0}L_i^{-1},\\ \label{eq:vpot}
&=&-\frac{G\!M\!m\!}{d} \Sigma^N_{i=0} \Sigma^{\infty}_{n=0}\! \left(\! \frac{r}{d}\! \right)^n
\!P_n\! \left(\! \cos{\!\left( \! \omega_{\mathrm{rot}} t \!+\!\frac{2 \pi i}{N}\right)\!}\right),
\end{eqnarray}
where $P_n$ is the Legendre polynomial, and $V_i$ is the potential of a mass. The equation of motion of the test mass is
\begin{eqnarray}
Ma&=&\left| \frac{\partial V}{\partial{d}} \right| =\frac{GMm}{d^2}\Sigma^N_{i=0} \Sigma^{\infty}_{n=0}(n+1) \left( \frac{r}{d} \right)^n \nonumber  P_n\left(\cos{\left(\omega_{\mathrm{rot}} t +\frac{2 \pi i}{N}\right)}\right),
\end{eqnarray}
where $a$ is the acceleration of the test mass.

We arrange the masses around the rotor in a superposition of quadrupole and hexapole arrangements, as shown in Fig.~\ref{fig:hex}. A hole is placed between each mass. These holes is effectively double the magnitude of the gravity gradient. Therefore, the equation of motion of the test mass is
\begin{eqnarray}
Ma&=&\left| \frac{\partial V}{\partial{d}} \right| =\frac{2GMm}{d^2}\Sigma^N_{i=0} \Sigma^{\infty}_{n=0}(n+1) \left( \frac{r}{d} \right)^n \nonumber P_n\left(\cos{\left(\omega_{\mathrm{rot}} t +\frac{2 \pi i}{N}\right)}\right). \label{eq:EOM}
\end{eqnarray}
Next, we will calculate the displacements of the quadrupole and hexapole rotor masses in sections ~\ref{Quad}  and ~\ref{Hexa}.

\begin{figure}
\begin{center}
\includegraphics[width=12cm]{Hexapole.eps}
\caption{Configuration of the rotor with quadrupole and hexapole mass distributions. $m_{\mathrm{q}}$ and $m_{\mathrm{h}}$ are the masses of quadrupole and hexapole masses. $r_{\mathrm{q}}$ and $r_{\mathrm{h}}$ are the radii of the quadrupole and arrangements hexapole.}
\label{fig:hex}
\end{center}
\end{figure}

\subsection{Displacement of test mass driven by quadrupole mass distribution} \label{Quad}
We calculate the displacement of the quadrupole mass distribution with two pieces and two holes so $N=2$.
The masses and radii of the quadrupole arrangement are $m_{\mathrm{q}}$ and $r_{\mathrm{q}}$.
The equation of motion for the test mass is
\begin{eqnarray}
Ma&=&\frac{2GMm_{\mathrm{q}}}{d^2}\Sigma^{\infty}_{n=0}(n+1) \left( \frac{r_{\mathrm{q}}}{d} \right)^n \nonumber  \Sigma^1_{i=0}  P_n\left(\cos{\left(\omega_{\mathrm{rot}} t +\pi i \right)}\right).
\end{eqnarray}
If we assume $r \ll d$, the displacement of the time-dependent lower harmonics can be written as
\begin{equation}
x=\Sigma_{k=1}^{\infty}x_{k\mathrm{f}}\cos(k\omega_{\mathrm{rot}} t)\sim x_{\mathrm{2f}}\cos(2\omega_{\mathrm{rot}} t)=x_{\mathrm{2f}}\cos{\omega t},
\end{equation}
where $k$ is the number of the harmonics.
The amplitude of the 2-f rotation is then
\begin{equation}
x_{2\mathrm{f}}=9\frac{GMm_{\mathrm{q}}r_{\mathrm{q}}^2}{d^4}s(\omega). \label{2f}
\end{equation}

\subsection{Displacement of test mass driven by hexapole mass distribution} \label{Hexa}
We also calculate the displacement of the hexapole mass distribution with three holes as $N=3$.
The masses and radii of the hexapole distribution are $m_{\mathrm{h}}$ and $r_{\mathrm{h}}$.
The equation of motion of test mass driven by this arrangement alone is
\begin{eqnarray}
Ma &=& \frac{2GMm_{\mathrm{h}}}{d^2}\Sigma^{\infty}_{n=0}(n+1) \left( \frac{r_{\mathrm{h}}}{d} \right)^n \nonumber  \Sigma^2_{i=0} P_n \left(\cos{\left(\omega_{\mathrm{rot}} t+\frac{2\pi i}{3} \right)} \right).
\end{eqnarray}
If we assume $r \ll d$, the displacement of the time-dependent lower harmonics can be written as
\begin{equation}
x=\Sigma_{k=1}^{\infty}x_{k\mathrm{f}}\cos(k\omega_{\mathrm{rot}} t)\sim  x_{3\mathrm{f}}\cos(3\omega_{\mathrm{rot}} t)=x_{\mathrm{3f}}\cos{\omega t},
\end{equation}
where amplitude of 3-f is described as
\begin{equation}
 x_{3\mathrm{f}}=15\frac{GMm_{\mathrm{h}}r_{\mathrm{h}}^3}{d^5}s(\omega). \label{3f}
\end{equation}

\section{Absolute power calibration with both photon and Gravity field calibrator} \label{sec:PGCAL}
This section discusses how to combine the calibration signals from Pcal and Gcal to allow absolute laser power calibration using an interferometer.
Figure~\ref{fig:IFO} diagrams the combined calibration system.
First, the test mass is driven by the Gcal. The $x_{\mathrm{2f}}$ and $x_{\mathrm{3f}}$ signals are measured from the response of the interferometer. Second, this interferometer signal is sent to the excitation port of the Pcal. This signal acts as a reference signal for feedback control, as shown in Fig.~\ref{fig:IFO}. The Pcal then cancels out the displacement modulated by the Gcal.
Third, the voltage responses of the transmitter and the receiver module photodetectors are measured. The output signal of the transmitter module, $V_{\mathrm{TxPD}}$ and receiver module, $V_{\mathrm{RxPD}}$ should correspond to the displacement caused by the Gcal. By using Eq~(\ref{eq:pcal}),(\ref{2f}), and (\ref{3f}), the modulated signal powers are
\begin{eqnarray}
 P_{\mathrm{2f}}=\frac{9}{2} \frac{Gcm_{\mathrm{q}}Mr_{\mathrm{q}}^2}{d^4cos\theta}\frac{1}{1+\frac{M}{I}\vec{a}\cdot \vec{b}}, \label{P2f} \\
 P_{\mathrm{3f}}= \frac{15}{2}\frac{Gcm_{\mathrm{h}}Mr_{\mathrm{h}}^3}{d^5cos\theta}\frac{1}{1+\frac{M}{I}\vec{a}\cdot \vec{b}}. \label{P3f}
\end{eqnarray}
Fourth, we demodulate the signal of the transmitter and receiver modules using the measured encoder signal from the Gcal.
The demodulated signals are
\begin{eqnarray}
V_{\mathrm{2f}}^{\mathrm{T}}=\rho_{\mathrm{T}}P_{\mathrm{2f}}, \\
V_{\mathrm{2f}}^{\mathrm{R}}=\rho_{\mathrm{R}}P_{\mathrm{2f}}, \\
V_{\mathrm{3f}}^{\mathrm{T}}=\rho_{\mathrm{T}}P_{\mathrm{3f}}, \\
V_{\mathrm{3f}}^{\mathrm{R}}=\rho_{\mathrm{R}}P_{\mathrm{3f}},
\end{eqnarray}
where $\rho_{\mathrm{T}}$ and $\rho_{\mathrm{R}}$ are the transfer functions from power to the photo detector output voltages at the transmitter and receiver modules.
Therefore, we can measure the distance from the ratio of responses of the 2-f and 3-f components:
\begin{equation}
d=\frac{5}{3} \frac{V_{\mathrm{2f}}^{\mathrm{T}}}{V_{\mathrm{3f}}^{\mathrm{T}}}\frac{m_{\mathrm{h}}}{m_{\mathrm{q}}}\frac{r_{\mathrm{h}}^{3}}{r_{\mathrm{q}}^{2}}=\frac{5}{3} \frac{V_{\mathrm{2f}}^{\mathrm{R}}}{V_{\mathrm{3f}}^{\mathrm{R}}} \frac{m_{\mathrm{h}}}{m_{\mathrm{q}}}\frac{r_{\mathrm{h}}^{3}}{r_{\mathrm{q}}^{2}}. \label{d}
\end{equation}

Finally, we calculate the displacement formula for the Pcal calibrated by Gcal. We substitute the Eq. (\ref{2f}) to  Eq. (\ref{eq:pcal}) to obtain the following equation for displacement:
\begin{eqnarray}
x&=&\frac{2P \cos{\theta}}{c} s(\omega)\left(1+\frac{M}{I}\vec{a} \cdot \vec{b} \right), \\
 &=&9\frac{Gm_{\mathrm{q}} M r_{\mathrm{q}}^2}{d^4}\frac{P}{P_{\mathrm{2f}}}s(\omega) , \\
 &=&\frac{729}{625} \frac{GM m^5_{\mathrm{q}} r_{\mathrm{q}}^{10}}{m^4_{\mathrm{h}} r_{\mathrm{h}}^{12} } \frac{{V_{\mathrm{3f}}^{R}}^4}{{V_{\mathrm{2f}}^{R}}^5}V_{\mathrm{in}} s(\omega)  , \label{pcal_new}
\end{eqnarray}
where we assumed that $P(\omega)=\rho_{\mathrm{R}} V_{\mathrm{in}}$, and $V_{\mathrm{in}}$ is the amplitude of the input voltage.
\begin{figure}
\begin{center}
\includegraphics[width=12cm]{IFO.eps}
\caption{Test apparatus for the absolute calibration. The Gcal is placed behind the test mass. The frequency of the Gcal is monitored with the encoder output. The error signal for the differential arm length of the interferometer is sent to the reference port of the photon calibrator for canceling the modulation of the dynamic gravity field with feedback with transfer function $G$. Output signals from the photon calibrator are synchronized with the forces driven by the Gcal. The output signals are demodulated with 2-f and 3-f signals monitored by the encoder.}
\label{fig:IFO}
\end{center}
\end{figure}
The factor $(GMm_{\mathrm{q}}^5 r_{\mathrm{q}}^{10})/(m_{\mathrm{h}}^4 r_{\mathrm{h}}^{12})$ can be measured before the calibration.  $V^R_{\mathrm{3f}}/V^R_{\mathrm{2f}}$ is measured during the calibration of the Gcal and Pcal. The interval of the calibration signals between the Pcal and Gcal depend on the stability of the photon calibrator laser power. The Advanced LIGO experiment calibrates the absolute laser power using the working standard monthly. Therefore, The Gcal should be run monthly or more frequently. The present method reconstructs the Pcal signal from Gcal signals.  Therefore, the Gcal does not need to be operated during observation runs.
During operation, the Gcal would contaminate the noise floor by adding acoustic and/or vibration noise. However, we can minimize this noise effect by controlling the rotation frequency. The above analysis has not considered to the noise added by the Gcal during observation runs, as we only propose that the Gcal be used to calibrate the absolute displacement before the observations.
The demodulation technique allows us to reduce the systematic error introduced by rotation . When the modulation of Gcal is canceled using  Pcal, the transfer functions of the Gcal and Pcal are also canceled. Therefore, the estimated displacement of the test mass does not depend on the frequency of the rotation.

\section{Estimation of uncertainty} \label{sec:EST}
In this section, we evaluate the accuracy of the estimated displacement, and discuss the effects on systematic error by changing the operating frequency and distance. After that, we discuss the uncertainty in the displacement of the mirror.
The following discussion assumes the basic parameters of the KAGRA experiment listed in Table~\ref{pcal}, and the parameters of the Gcal as listed in Table~\ref{sus}.

\begin{table}
\begin{center}
\caption{\label{sus}Assumed parameters. $G$ is gravity constant~\cite{RevModPhys.88.035009}. $\theta$ is incident angle of the Pcal beams. $M$ is mass of test mass. $1+\frac{I}{M}\vec{a}\cdot \vec{b}$ is geometrical factor.}
\footnotesize
\begin{tabular}{ccc}
\hline
&Value&Relative uncertainty \\
\hline
$G$&$6.67408 \times 10^{-11}~\mathrm{m^3kg^{-1}sec^{-2}}$&0.0047 \%\\
$\cos{\theta}$ &1.000& 0.07~\%\\
$M$ &22.89~kg & 0.02~\%\\
$m_{\mathrm{q}}$&4.485~kg & 0.004~\%\\
$m_{\mathrm{h}}$& 4.485~kg &0.004~\%\\
$r_{\mathrm{q}}$&0.200~m & 0.010~\%\\
$r_{\mathrm{h}}$& 0.125~m & 0.016~\%\\
$1+\frac{I}{M}\vec{a}\cdot \vec{b}$& 1&0.3~\% \\
\hline
\end{tabular}\\
\end{center}
\end{table}

\subsection{Systematic error of higher order terms}
To achieve the precision less than 1 \%, we need to consider the effect of higer-order Legendre polynomials at the position of the test mass. This is because higher-order polynomials also affect the 2-f and 3-f components. The $n$-th order Legendre polynomial is calculated with Eq.(\ref{eq:EOM}). The effect of higher-order factors is mitigated by the factor $(r/d)^n$. Tables~\ref{tab:N2} and \ref{tab:N3} show the calculated displacements of the higher order terms.
To investigate the higher order effects, we compare the estimated test mass displacement between the Legendre polynomial approximation and numerical calculations of $\frac{\partial V}{\partial{d}}$ and Eq.(\ref{eq:vpot}). The ratio of two calculations of the test mass displacement is shown in Figs.~\ref{fig:FEM-2f} and ~\ref{fig:FEM-3f} for the quadrupole ($N=2$) and hexapole ($N=3$) components, respectively, as a function of the distance, $d$.
The results show that the effect of higher-order of polynomials is less than that of systematic error. The mirror therefore needs to be placed at least 2~m away from the rotating mass. Then the sum of the first and second order equations can be used to suppress the systematic error well below 1 \% as shown in Figs.~\ref{fig:FEM-2f} and \ref{fig:FEM-3f}.
If we place the Gcal near the KAGRA end test mass, the distance of 2~m is reasonable. The rotor could be mounted outside of the vacuum chamber. In the following calculations, we assume $d= $~2~m for the simplification of the discussion.
The analytical calculation of the displacement of the test mass in Eq.(\ref{eq:EOM}) assumes that the rotor masses and the test mass can be approximated as point masses.
We compared the results of this analytical calculation with the numerical integral of the displacements generated by the actual dimensions of the rotor
with the parameters shown in Table~\ref{sus}, and confirmed that the analytical formula is sufficiently at $d= $~2~m.

\begin{table}
\begin{center}
\caption{Calculated quadrupole ($N=2$) displacement. $n$ is the order of the Legendre polynomial, where $\omega=n\omega_{\mathrm{rot}}$. \label{tab:N2}}
\footnotesize
\begin{tabular}{cccccccc}
\hline
& n=1 & n=2& n=3 &n=4&n=5&n=6&n=7 \\
\hline
1-f&0&0&0&0&0&0&0 \\
2-f&0&$9 \frac{Gmr^2}{d^4\omega^2}$&0&$\frac{25}{4} \frac{Gmr^4}{d^6\omega^2}$&0&$\frac{735}{128} \frac{Gmr^6}{d^8\omega^2}$&0  \\
3-f&0&0&0&0&0&0&0\\
4-f&0&0&0&$\frac{175}{16} \frac{Gmr^4}{d^6\omega^2}$&0& $\frac{273}{32} \frac{Gmr^6}{d^8\omega^2}$&0 \\
5-f&0&0&0&0&0&0&0 \\
6-f&0&0&0&0&0&$\frac{1617}{128} \frac{Gmr^6}{d^8\omega^2}$&0  \\
\hline
\end{tabular}
\end{center}
\end{table}

\begin{table}
\begin{center}
\caption{Calculated hexapole ($N=3$) displacement. $n$ is the order of the Legendre polynomial, where $\omega=n\omega_{\mathrm{rot}}$.  \label{tab:N3}}
\footnotesize
\begin{tabular}{cccccccc}
\hline
& n=1 & n=2& n=3 &n=4&n=5&n=6&n=7 \\
\hline
1-f&0&0&0&0&0&0&0 \\
2-f&0&0&0&0&0&0&0  \\
3-f&0&0&$15\frac{Gmr^3}{d^5\omega^2}$&0&$\frac{315}{32}\frac{Gmr^5}{d^7\omega^2}$&0& $\frac{567}{64} \frac{Gmr^7}{d^9 \omega^2}$\\
4-f&0&0&0&0&0&0&0 \\
5-f&0&0&0&0&0&0&0 \\
6-f&0&0&0&0&0&$\frac{4851}{256} \frac{Gmr^6}{d^8\omega^2}$&0  \\
\hline
\end{tabular}
\end{center}
\end{table}

\begin{figure}
\begin{center}
\includegraphics[width=12cm]{2f.eps}
\caption{Ratio of Legendre polynomial approximations with the numerical calculations of $\frac{\partial V}{\partial{d}}$ and Eq.(~\ref{eq:vpot})
on the test mass displacement for the quadrupole ($N=2$) component as a function of the distance. Dotted, dashed and solid lines correspond to first-order only, second-orders, and third-order approximations, respectively.
The analytical results are listed in Table~\ref{tab:N2}. To achieve precision less than 1~\%, the higher-order terms need to be included.}
\label{fig:FEM-2f}
\end{center}
\end{figure}

\begin{figure}
\begin{center}
\includegraphics[width=12cm]{3f.eps}
\caption{Ratio of the Legendre polynomial approximation to the numerical calculations of $\frac{\partial V}{\partial{d}}$ and Eq.(~\ref{eq:vpot})
on the test mass displacement for the hexapole distribution ($N=3$) component as a function of distance. The dotted, dashed and solid lines correspond to the first-order only, second-orders, and third-orders, respectively.
The analytical result is listed in Table~\ref{tab:N3}. To achieve the precision less than 1~\%, the higher-order terms need to be included..}
\label{fig:FEM-3f}
\end{center}
\end{figure}

\subsection{Systematic error of the transfer function}
The Gcal modulates the test mass mirror with gravitational potential gradient. However, this gradient also actuates the masses of suspension system as shown in Fig.~\ref{fig:cryo}. We simulated the transfer function with the assumption of the cryogenic suspension system installed in KAGRA~\cite{0264-9381-34-22-225001}.The transfer function was calculated using the rigid-body suspension simulation code, called SUMCON~\cite{SUMCON}. We estimated the total displacement by superimposing the displacements driven by both mass distributions. Figure \ref{fig:ratio} shows the displacement ratio between the motion signal and the free-mass motion as a function of frequency. The simulation result is in good agreement with the free-mass motion at this frequencies larger than 20~Hz. The low frequency structures correspond to the resonant peak of the suspension system. Therefore, we can neglect this intermediate-mass effect and regard as motion at frequency over 20~Hz as free-mass motion.
Therefore, we need to operate the rotor at speeds larger than 20 Hz to achieve error less than 0.1~\%.
We assumed the rotation frequency to be 16~Hz, which corresponds to 32~Hz and 48~Hz for the effective frequency of the 2-f and 3-f components.
This assumption applies to the discussion in the next section.

\begin{figure}
\begin{center}
\includegraphics[width=12cm]{Cryo.eps}
\caption{Schematic of the suspension system. The parameters of the heights and masses are marked with their assumed values. }
\label{fig:cryo}
\end{center}
\end{figure}

\begin{figure}
\begin{center}
\includegraphics[width=12cm]{dx_Gcal_ratio.eps}
\caption{Displacement ratio of the transfer function for mult-pendulums by changing modulation frequency. The relations of the modulation frequency, $f$, modulation angular frequency, $\omega$, and rotation angular frequency $\omega_{\mathrm{rot}}$ are described as $n\omega_{\mathrm{rot}}=\omega=2\pi f$. }
\label{fig:ratio}
\end{center}
\end{figure}

\subsection{Uncertainty of displacement and  laser power}
In this section, we estimate the typical displacement based on the result in Table.~\ref{sus}. We neglect Legendre polynomials of degree higher than twwo in the following discussion to simplify the discussion, though they are relevant in the calculations.
 The estimated 2-f and 3-f displacements are described as
 \footnotesize
\begin{eqnarray}
x^{\mathrm{rms}}_{\mathrm{2f}}&=&1.18 \times 10^{-16}\mathrm{[m]} \times \left( \frac{G}{6.67408 \times 10^{-11} \mathrm{[m^3kg^{-1}sec^{-2}]}} \right) \nonumber \\
&\times&\! \left( \! \frac{m_{\mathrm{q}}}{4.485 \mathrm{[kg]}} \!\right) \! \times \!\left( \!\frac{r_{\mathrm{q}}}{0.200 \mathrm{[m]}} \! \right)^2 \! \times \! \left( \! \frac{2\mathrm{[m]}}{d} \! \right)^4 \! \times \! \left( \! \frac{2\pi \! \times \! 32\mathrm{[Hz]}}{\omega} \! \right)^2,\\
x^{\mathrm{rms}}_{\mathrm{3f}}&=&2.13 \times 10^{-18}\mathrm{[m]} \times \left( \frac{G}{6.6742 \times 10^{-11} \mathrm{[m^3kg^{-1}sec^{-2}]}} \right) \nonumber \\
&\times& \! \left( \! \frac{m_{\mathrm{h}}}{4.485 \mathrm{[kg]}}\! \right) \! \times \! \left(  \!\frac{r_{\mathrm{h}}}{0.125 \mathrm{[m]}} \! \right)^3
\! \times \! \left(\! \frac{2\mathrm{[m]}}{d} \! \right)^5 \! \times \! \left( \! \frac{2\pi\!\times \! 48\mathrm{[Hz]}}{\omega} \! \right)^2.
\end{eqnarray}
\normalsize

We define the SNR in the term of the ratio of RMS displacement of the design noise spectrum density for the interferometer of KAGRA at 32~Hz for 2-f and 48~Hz for 3-f.
Using this result, we estimate the SNR of the peaks.

\footnotesize
\begin{eqnarray}
\!S\!N\!R_{\mathrm{2f}}&=&392 \times \left(\frac{3.0 \times 10^{-19} [\mathrm{m/\sqrt{Hz}}]}{n_{\mathrm{32Hz}}} \right)  \times \left(\frac{T}{1 [\mathrm{sec}]} \right)^{\frac{1}{2}} \left(\frac{x_{\mathrm{2f}}^{\mathrm{rms}}}{1.178 \times 10^{-16}\mathrm{[m]} }  \right),   \\
\!S\!N\!R_{\mathrm{3f}}&=&73 \times \left(\frac{2.9 \times 10^{-20} [\mathrm{m/\sqrt{Hz}}]}{n_{\mathrm{48Hz}}} \right) \times \left(\frac{T}{1 [\mathrm{sec}]} \right)^{\frac{1}{2}} \left(\frac{x_{\mathrm{2f}}^{\mathrm{rms}}}{2.130 \times 10^{-18}\mathrm{[m] }} \right),
\end{eqnarray}
\normalsize
where $T$ is the integration time. If we integrate a signal larger than 3 min, we can measure $V^{\mathrm{R}}_{2f}$ and $V^{\mathrm{R}}_{3f}$ with sufficiently high SNR that systematic error can be reduced to less than 0.1~\%.

This method used to measure the absolute laser power as well. The estimated powers are
\footnotesize
\begin{eqnarray}
P_{\mathrm{2f}}&=&0.023 ~\mathrm{[W]}\times \left( \frac{G}{6.6742 \times 10^{-11} \mathrm{[m^3kg^{-1}sec^{-2}]}} \right) \times \left( \frac{m_{\mathrm{q}}}{4.485 \mathrm{[kg]}} \right) \times \left( \frac{r_{\mathrm{q}}}{0.200 \mathrm{[m]}} \right)^2 \times \left( \frac{2\mathrm{[m]}}{d} \right)^4 \nonumber \\ &&\times \left( \frac{1}{\cos{\theta}} \right) \times \left( \frac{1}{1+\frac{M}{I}\vec{a}\cdot \vec{b}} \right)^2,\\
P_{\mathrm{3f}}&=&0.00095~\mathrm{[W]} \times \left( \frac{G}{6.6742 \times 10^{-11} \mathrm{[m^3kg^{-1}sec^{-2}]}} \right) \times \left( \frac{m_{\mathrm{h}}}{4.485 \mathrm{[kg]}} \right) \times \left( \frac{r_{\mathrm{h}}}{0.125 \mathrm{[m]}} \right)^3 \times \left( \frac{2\mathrm{[m]}}{d} \right)^5 \nonumber \\ &&\times \left( \frac{1}{\cos{\theta}} \right) \times \left( \frac{1}{1+\frac{M}{I}\vec{a}\cdot \vec{b}} \right)^2.
\end{eqnarray}
\normalsize
We estimate the laser power with following equations:
\footnotesize
\begin{eqnarray}
\left( \frac{\delta P_{\mathrm{2f}}}{P_{\mathrm{2f}}} \right)^2 &\sim&  \!16 \! \left( \frac{\delta V^{\mathrm{R}}_{{\mathrm{2f}}}}{V^{\mathrm{R}}_{{\mathrm{2f}}}} \!\right)^2+16\left( \frac{\delta V^{\mathrm{R}}_{{\mathrm{3f}}}}{V^{\mathrm{R}}_{{\mathrm{3f}}}} \right)^2 +\left( \frac{\delta P_{\mathrm{sys}}}{P_{\mathrm{sys}}} \right)^2, \label{dP2f} \\
\left( \frac{\delta P_{\mathrm{3f}}}{P_{\mathrm{3f}}} \right)^2 &\sim&  \!16 \! \left( \frac{\delta V^{\mathrm{R}}_{{\mathrm{2f}}}}{V^{\mathrm{R}}_{{\mathrm{2f}}}} \right)^2+16\left( \frac{\delta V^{\mathrm{R}}_{{\mathrm{3f}}}}{V^{\mathrm{R}}_{{\mathrm{3f}}}} \right)^2+\left( \frac{\delta P_{\mathrm{sys}}}{P_{\mathrm{sys}}} \right)^2,  \label{dP3f}
\end{eqnarray}
\normalsize
where $\delta P_{\mathrm{sys}}/P_{\mathrm{sys}}$ is the relative systematic error of the power due to the machining tolerance of the rotor masses and radiuses, which are calculated by
\begin{eqnarray}
\frac{\delta P_{\mathrm{sys}}}{P_{\mathrm{sys}}}&\sim& \frac{\delta G}{G} + \frac{\delta M}{M} +\frac{\delta \cos{\theta}}{\cos{\theta}}+ \frac{\delta\left( 1+\frac{M}{I}\vec{a}\cdot \vec{b} \right)}{\! \left( \! 1+\frac{M}{I}\vec{a}\cdot \vec{b} \! \right)}
+\frac{12}{\sqrt{6}} \frac{\delta r_{\mathrm{h}}}{r_{\mathrm{h}}} +\frac{10}{2} \frac{\delta r_{\mathrm{q}}}{r_{\mathrm{q}}}  +\frac{5}{2} \frac{\delta m_{\mathrm{q}}}{m_{\mathrm{q}}} +\!\frac{4}{\sqrt{6}}  \! \frac{\delta m_{\mathrm{h}}}{m_{\mathrm{h}}}.
\end{eqnarray}
 We next consider the mitigating effect of the systematic error of the masses and radiuses due to the tolerance and uncertainty of the measurement instruments. The values of the masses and radiuses vary slightly with the tolerance of the fabrication process. The errors in $m_{\mathrm{q}}$, $r_{\mathrm{q}}$, $m_{\mathrm{h}}$, and $r_{\mathrm{h}}$ are mitigated by the factor of $1/\sqrt{6}$ and $1/\sqrt{4}$.
The uncertainty in the quadrupole and hexapole masses are limited by the accuracy of the electronic balance. In this case, we modeled masses made of Tungsten. The density of Tungsten is $19.25~\mathrm{g/cm^3}$. The diameter and thickness of the mass are 0.06~m and 0.08~m, respectively. Therefore, the mass of the rotor mass is 4.485~kg. We assumed that the CG-6000 electronic balance is used to weigh these means, with tolerance of 0.2~g~\cite{CG6000}. Therefore, the relative uncertainty in the mass of the rotor mass is 0.004~\%.

 The rotor disk can be machined by Numerical Control milling. Dimensional accuracy
of less than 0.02 mm can typically be achieved with this process. For measuring the shape, we assume that a three-dimension coordinate measuring machine (CMM) will be employed~\cite{Inoue:16}. The precision of CMM is $2~\mathrm{\mu m}$. This indicates that we can measure the shape of the rotor and masses with  sufficiently low uncertainty using the CMM.

The estimated relative uncertainties of the laser powers are 0.52~\%. One of the largest uncertainties is the geometrical factor of the Pcal laser. The geometrical factor uncertainty is assumed to be 0.3 \%, which is the same number as the instrument used in Advanced LIGO.

Finally, assuming that the statistical fluctuations of $V_{in}$, $s(\omega)$, $V^{\mathrm{R}}_{{\mathrm{2f}}}$, and $V^{\mathrm{R}}_{{\mathrm{3f}}}$ are independent for each measurement and therefore can be added in quadrature, the estimated relative uncertainty in the displacement measurements is written as
 \footnotesize
\begin{equation}
\left( \frac{\delta x}{x} \right)^2 \!\sim \! \left( \!\frac{\delta V_{in}}{V_{in}}\! \right)^2+\left(\! \frac{\delta s(\omega)}{s(\omega)} \! \right)^2\!+\!25\!\left(\!\frac{\delta V^{\mathrm{R}}_{{\mathrm{2f}}}}{V^{\mathrm{R}}_{{\mathrm{2f}}}}\! \right)^2+16\!\left(\! \frac{\delta V^{\mathrm{R}}_{{\mathrm{3f}}}}{V^{\mathrm{R}}_{{\mathrm{3f}}}}\! \right)^2\!+ \left(\! \frac{\delta x_{\mathrm{sys}}}{x_{\mathrm{sys}}} \! \right)^2 \label{deltax},
\end{equation}
\normalsize
where $\delta x_{\mathrm{sys}}/x_{\mathrm{sys}}$ is the relative systematic error of the displacement which cannot be added in quadrature. This factor is written as
 \footnotesize
\begin{equation}
\frac{\delta x_{\mathrm{sys}}}{x_{\mathrm{sys}}}=\frac{\delta G}{G} + \frac{\delta M}{M} +\frac{12}{\sqrt{6}} \frac{\delta r_{\mathrm{h}}}{r_{\mathrm{h}}} +\frac{10}{2} \frac{\delta r_{\mathrm{q}}}{r_{\mathrm{q}}}  +\frac{5}{2} \frac{\delta m_{\mathrm{q}}}{m_{\mathrm{q}}} +\!\frac{4}{\sqrt{6}}  \! \frac{\delta m_{\mathrm{h}}}{m_{\mathrm{h}}}.
\end{equation}
\normalsize
We assumed the mitigation factors of radiuses and masses discussed above in this calculation.
To reduce the noise of the displacement measurement, we need to reduce the uncertainty in the shape of the rotor and masses.
The uncertainties in $V^{\mathrm{R}}_{\mathrm{2f}}$,$V^{\mathrm{R}}_{\mathrm{3f}}$, $V^{\mathrm{R}}_{0}$ are much less than that of other contributions. We can reduce the uncertainty of these values using long integration times with statistical measures. Each of the uncertainty is listed in Table~\ref{sus}. The estimated  total uncertainty of the displacement measurement is 0.17~\%.

\section{Conclusion}
Pcal are used in Advanced LIGO, Advanced Virgo and KAGRA. These devices are used to calibrate the interferometer response, and the uncertainty in the calibration affects the estimation of parameters of the GW source. In particular, the distance to the source strongly depends on the absolute laser power of the photon calibrator. In previous studies, the gold standard, in which the interferometer response is calibrated to the NIST laser power standard, was used for the absolute laser power calibration of the photon calibrator. However, the current standard for absolute laser power vary by a few~\% between different countries's metrology institutes. This uncertainty propagates directly to the calculation of the GW detector's absolute displacement.
To address this problem, we proposed a combined calibration method that uses both a Pcal and a Gcal. The Gcal modulated the test mass using a dynamic gravity field. When canceling the displacement of the test mass using the Pcal, the Gcal was used to calibrate the interferometer responce.

This method had the advantage of offering a direct comparison between the amplitudes of the injected power and gravity field modulation at the test mass. Without the proposed gravity-field calibrator, the uncertainties of the optical efficiency through the window and mirrors and the geometrical factor of the laser position need to considered, because the working standard calibration is measured outside of the chamber. However, the method of gravity field can compare the displacement directly. Using this method, the uncertainty of the optical efficiency is avoided when calibrating the absolute laser power. The estimated laser power uncertainty with this method is 0.52~\%. This result suggests that a new power calibration standard can be proposed that gains threefold improvement over the current standards.

Finally, we estimated the uncertainty of absolute calibration with the proposed method. The estimated absolute uncertainty in the displacement measurement is 0.17~\%, which is a tenfold improvement on previous studies. This uncertainty affects the estimation of the distance to the gravitational wave source. This estimated uncertainty brings the precision of the Hubble constant to less than 1~\%. This may address the tension between the Cephied-SN distance ladder~\cite{Riess_2016} and CMB data assuming a $\Lambda$CDM
model~\cite{2016-planck}.

\acknowledgments

We thank Richard Savage and Darkhan Tuyrnbayev for discussion of the photon calibrator. We would like to express our gratitude to Prof. Takaaki Kajita and Prof. Henry Wong. We would like to thank the KEK Cryogenics Science Center for the support. YI and SH are supported by Academia Sinica and Ministry of Science and Technology (MOST) under Grants No. CDA-106-M06, MOST106-2628-M-007-005 and MOST106-2112-M-001-016 in Taiwan. This work was supported by JSPS KAKENHI Grant Numbers 17H106133 and 17H01135. KAGRA project is supported by MEXT, JSPS Leading-edge Research Infrastructure Program, JSPS Grant-in-Aid for Specially Promoted Research 26000005, MEXT Grant-in-Aid for Scientific Research on Innovative Areas 24103005, JSPS Core-to-Core Program, A. Advanced Research Networks, and the joint research program of the Institute for Cosmic Ray Research, University of Tokyo.

redpajama_set_name: RedPajamaArXiv


text:
A Passion for Paris
Romanticism and Romance in the City of Light
David Downie
MP3 CD (5/31/2016)
"A top-notch walking tour of Paris. . . . The author's encyclopedic knowledge of the city and its artists grants him a mystical gift of access: doors left ajar and carriage gates left open foster his search for the city's magical story. Anyone who loves Paris will adore this joyful book. Readers visiting the city are advised to take it with them to discover countless new experiences." —Kirkus Reviews (starred)
A unique combination of memoir, history, and travelogue, this is author David Downie's irreverent quest to uncover why Paris is the world's most romantic city—and has been for over 150 years.
Abounding in secluded, atmospheric parks, artists' studios, cafes, restaurants and streets little changed since the 1800s, Paris exudes romance. The art and architecture, the cityscape, riverbanks, and the unparalleled quality of daily life are part of the equation.
But the city's allure derives equally from hidden sources: querulous inhabitants, a bizarre culture of heroic negativity, and a rich historical past supplying enigmas, pleasures and challenges. Rarely do visitors suspect the glamor and chic and the carefree atmosphere of the City of Light grew from and still feed off the dark fountainheads of riot, rebellion, mayhem and melancholy—and the subversive literature, art and music of the Romantic Age.
Weaving together his own with the lives and loves of Victor Hugo, Georges Sand, Charles Baudelaire, Balzac, Nadar and other great Romantics Downie delights in the city's secular romantic pilgrimage sites asking , Why Paris, not Venice or Rome—the tap root of "romance"—or Berlin, Vienna and London—where the earliest Romantics built castles-in-the-air and sang odes to nightingales? Read A Passion for Paris: Romanticism and Romance in the City of Light and find out.
Praise For A Passion for Paris: Romanticism and Romance in the City of Light…
"If you're interested in colorful history and literature, A Passion For Paris is the book for you. Read it before you visit or return to the city-you'll be the richer for it." —Rudy Maxa, Host of America's #1 travel radio show, "Rudy Maxa's World"
"From its alleys and ateliers to its cafes and cathedrals, Downie crafts an infatuated valentine to the City of Light" —National Geographic Traveler Magazine
"I want to highly recommend a book... We can never get enough of Paris!" —Liz Smith, NewYorkSocialDiary.com
"150 years' worth of reasons why the city merits the epithet." —Journeys magazine
"A top-notch walking tour of Paris… Downie is the consummate guide…The author's encyclopedic knowledge of the city and its artists grants him a mystical gift of access: doors left ajar and carriage gates left open foster his search for the city's magical story. Anyone who loves Paris will adore this joyful book. Readers visiting the city are advised to take it with them to discover countless new experiences." —Kirkus, STARRED review
"[I]intrepidly researched, entrancingly descriptive, ruminative, funny, and revealing... Downie presents a gorgeously discursive and affecting homage to Paris' 'great Romantics,' and to the city itself" —Booklist, STARRED review
"Paris has been cherished, admired, analyzed for centuries, yet in his wildly entertaining, operatic A Passion for Paris, David Downie seems to offer up a whole new place. Writing with an engaging informality, he delves into this most romantic of cities, then and now, focusing particularly on the Romantic Age and its people. . . . Whether the author is leading us into Flaubert's study or onto the terrace of today's Deux Magots, there's a rare excitement in the air--as if Puccini's Bohemians were united in song, somewhere off stage." —Penelope Rowlands, author of Paris Was Ours
"Victor Hugo, Adèle and Juliette, Saint-Beuve, Nadar, George Sand and a host of other great figures of French history come alive in David Downie's compelling and often wickedly humorous investigation of romance and romanticism in the City of Light. Most travelers agree that Paris is by far the most romantic city in the world but thanks to Downie's extensive research, passionate sleuthing and inspired imagination, they'll now know why. This unusual and exquisitely told tale of French romanticism is a must-read for true Paris lovers." —Harriet Welty Rochefort, author of French Toast and Joie de Vivre
"An entertaining read. David Downie is fabulous company!" —Jacki Lyden, "All Things Considered," NPR on On Paris to the Pyrenees
"Downie's adroit, learned, and ambitious book reinvigorates my sense of travel, taking me back to the happy knowledge that the world is still large, and history unfathomably deep." —Frances Mayes, author of Under the Tuscan Sun on On Paris to the Pyrenees
"David Downie is the master of educated curiosity. I have walked some of the city's streets with him, and reading this book is just as tactile an experience." —Michael Ondaatje on Paris, Paris
St. Martin's Press, 9781250043153, 320pp.
DAVID DOWNIE, a native San Franciscan, lived in New York, Providence, Rome and Milan before moving to Paris in the mid-80s. He divides his time between France and Italy. His travel, food and arts features have appeared in leading print and on-line publications including Bon Appétit, Gourmet, Saveur, Epicurious.com, and Gault & Millau, the premier French food guide. He is the author of over a dozen nonfiction books, including the highly acclaimed Paris, Paris and A Passion for Paris.


text:
Q: Value of i for (i == -i && i != 0) to return true in Java I have the following if condition.
if (i == -i && i != 0)

What value of i will return true for this condition in Java?
I am unable to think of any such value of i considering two's complement notation in Java.
I would also love to have algebraic proof of whatever answer this condition has (in context with Java)?

A: Tentative algebraic proof, using modulo 2^32 arithmetic:
i == -i can be rewritten as 2 * i == 0 (adding i on both sides), or i << 1 == 0.
This equation has two solutions of the form i == 0 >> 1, namely 0b and 10000000000000000000000000000000b obtained by shifting in either 0 or 1 on the left.
The solution i == 0 being excluded, there remains the solution i == 100000000000000000000000000000000b.

A: The value you are looking for is Integer.MIN_VALUE.

I would also love to have algebraic proof of whatever answer this condition has(in context with java)?

That's off-topic for Stack Exchange.  But you could do it starting from the definition of Java integers (JLS 4.2)

"The integral types are byte, short, int, and long, whose values are 8-bit, 16-bit, 32-bit and 64-bit signed two's-complement integers ..."

and

"The values of the integral types are integers in the following ranges ...
      For int, from -2147483648 to 2147483647, inclusive"

and the definition of the Java unary '-' operator (JLS 15.15.4):

"For integer values, negation is the same as subtraction from zero. The Java programming language uses two's-complement representation for integers, and the range of two's-complement values is not symmetric, so negation of the maximum negative int or long results in that same maximum negative number. Overflow occurs in this case, but no exception is thrown. For all integer values x, -x equals (~x)+1."

A: In additional to the answers given so far...
There is four values in total
int i = Integer.MIN_VALUE;
long i = Long.MIN_VALUE;
Integer i = Integer.valueOf(Integer.MIN_VALUE);
Long i = Long.valueOf(Long.MIN_VALUE);

The wrapped values get unwrapped so they are also true for this expression.
Note: Math.abs documents.

public static int abs(int a)
Returns the absolute value of an int
  value. If the argument is not negative, the argument is returned. If
  the argument is negative, the negation of the argument is returned.
Note that if the argument is equal to the value of Integer.MIN_VALUE,
  the most negative representable int value, the result is that same
  value, which is negative.

and

public static long abs(long a)
Returns the absolute value of a long value. If the argument is not
  negative, the argument is returned. If the argument is negative, the
  negation of the argument is returned.
Note that if the argument is equal to the value of Long.MIN_VALUE, the
  most negative representable long value, the result is that same value,
  which is negative.

It is surprising that Math.abs might return a negative number.  This happens either because a) there is no positive values for -MIN_VALUE in these cases b) performing the - calculation results in an overflow.
What is also interest is why doesn't Byte.MIN_VALUE, Short.MIN_VALUE do not do this.  This is because the - changes the type to int for these and thus no overflow.
Character.MIN_VALUE doesn't have a problem because it is 0.
Float.MIN_VALUE and Double.MIN_VALUE have a different meaning.  These are the smallest representable value greater than zero. Thus they have valid negative values which are not themselves.

A: Like the others have mentioned, this is only fulfilled by Integer.MIN_VALUE. As for proof, let me offer an easier to understand explanation other than in binary (although it is still rooted in that).
Note that Integer.MIN_VALUE is equal to -2^31 or -2147483648 and Integer.MAX_VALUE is equal to 2^31-1 or 2147483647. -Integer.MIN_VALUE is 2^31, which is now too large for an Integer (since it is past MAX_VALUE) thus causing an Integer overflow, making it Integer.MIN_VALUE again. It's the only Integer that does this since MIN_VALUE is the only number with no negative equivalent aside from 0.

A: The only int value for which it works is  Integer.MIN_VALUE.
It's because integers are negated using the two's complement way.
Using
System.out.println(Integer.toBinaryString(Integer.MIN_VALUE));

you see that Integer.MIN_VALUE is
10000000000000000000000000000000

Taking the negative value is done by first swapping 0 and 1, which gives
01111111111111111111111111111111

and by adding 1, which gives
10000000000000000000000000000000

As you can see in the link I gave, Wikipedia mentions the problem with the most negative numbers and specifies it's the sole exception :

The most negative number in two's complement is sometimes called "the
  weird number," because it is the only exception.

Of course you have the same phenomenon for Long.Min_Value if you store it in a long variable.
Note that this is only due to choices that were made regarding the binary storage of ints in Java. Another (bad) solution could for example have been to negate by simply changing the most significant bit and letting the other bits unchanged, this would have avoided this problem with MIN_VALUE but would have made 2 different 0 values and complicated binary arithmetic (how would you have incremented for example ?).

A: Maybe it's not too educative, but instead of thinking you could run this code:
    for (int i = Integer.MIN_VALUE; i <= Integer.MAX_VALUE; i++)
    {
        if (i == -i && i != 0)
        {
            System.out.println(i);
        }
    }

to see that it prints
-2147483648
-2147483648

infinitely :)


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text:
Twilight Begins
Wings in the Night
Maggie Shayne
fantasy, romance > paranormal romance
An omnibus edition Twilight Phantasies and Twilight Memories.
Genres: fantasy, romance > paranormal romance
New York Times and USA Today bestselling, RITA® Award winning Author Maggie Shayne published 62 novels and 22 novellas for five major publishers over the course of 22 years. She also spent a year writing for American daytime TV dramas Guiding Light and As the World Turns, and was offered the position of co-head writer of the former; an offer she tearfully turned down. It was scary, turning down an offer that big. But in March 2014, she did something even scarier. She left her job with the world's largest publisher, and went "indie." And it has gone so well that by July 2015 she had incorporated her new business, Thunderfoot Publishing Inc. She's never enjoyed her career more.
This new frontier of publishing is bringing
Maggie success like she's never seen in three distinct areas of her work. First, her contemporary western romances, The Texas Brands series and the Oklahoma All-Girl Brands. Secondly, her romantic thrillers, Brown and de Luca, her Shattered Sisters Series, and so on. And thirdly, her beloved paranormals, including the Wings in the Night series, which has the distinction of being the second vampire romance novel series ever, launching just a year after Lori Herter's Obsession series created a new genre; paranormal romance. All three of these sub-genres have a found a new and enthusiastic audience with the advent of ebooks and independent publishing.
Wings in the Night :: Series


Accvent holding company: A relatively new company established in the United States of America, Accvent decided to acquire ownership interests in three cutting-edge technology companies headquartered in Miami. Focused on innovation and collaboration with Klip Xtreme, Nexxt Solutions, Forza, Xtech and Primus, Accvent seeks to provide innovative results through this strategic partnership, for the successful consolidation as leaders in each particular market in which these three corporations currently participate.
Accvent vision is to broaden its scope to encompass a significant share of the fast growing technology industry on a global scale, with distribution channels in the USA, Latin America, the Caribbean and recently, in South Africa. Using experience, tradition and expertise in this highly diversified field of technology, Accvent is consistently lending its assistance to improve coordination among its strategic business units --now under the umbrella of a holding company-- in order to achieve each brand's corporate goals and to continue the expansion of their operations worldwide.


The eCommerce Minute is your daily dose of eCommerce, tech and retail news, with your hosts Bart Mroz and John Suder. The show is a production of SUMO Heavy, an eCommerce consulting firm with offices in Brooklyn, NY, and Philadelphia. Become a supporter of this podcast: https://anchor.fm/ecommerceminute/support.
Meal kit convenience comes with a massive downside. A typical meal kit delivery comes with insulation, gel-filled icepacks, and tiny lil containers or bags holding individual ingredients–like a few sprigs of herbs or a few spoonfuls of sauce or condiments –all this inside a giant cardboard box.
The Liviri containers eliminate single-use packaging and can be reused up to 75 times.


text:
Home News Analysis Anonymous Vs. the Zetas
Anonymous Vs. the Zetas
Geoffrey Ramsey
Zetas
After initial mixed signals, it appears that online hacker collective Anonymous has decided to take on Mexico's most violent and feared drug cartel, the Zetas, which could put the drug gang in a tight spot.
In just the past few days, rumors of a showdown between Anonymous and the Zetas drug cartel have been the subject of a veritable media frenzy. Speculation about the scope of the confrontation abounds, fueled by several conflicting reports about the "hacktivist" group's intentions.
The source of the confusion is a YouTube video (embedded below) which was posted on October 6 by one "MrAnonymousguyfawkes," which shows a masked speaker accusing the Zetas in Veracruz of having kidnapped a member of Anonymous in that state. As retribution, the individual claims that Anonymous will expose Zetas-linked police officers, officials and journalists unless their associate is released. "You made a great mistake in taking one of us; release him and if something happens to him, you [expletive] will remember the 5th of November."
The ultimatum received little attention from Mexican media until STRATFOR picked up on the story and published an analysis of the incident. In their report, the global intelligence company points out that any individual that Anonymous names as a Zetas collaborator will likely be killed, "whether or not the information released is accurate." The report also notes that the move opens up the hackers to reprisal attacks, as the Zetas have been known to target their online critics in the past. Three individuals were tortured and killed in Nuevo Laredo in two separate incidents in September, with signs left next to the bodies accusing them of reporting crimes on Internet forums.
As news of Anonymous' threat spread, they appeared to make their first move on October 28, when the group defaced the website of Gustavo Rosario Torres, a former state prosecutor from Tabasco. The page, which remained vandalized at the time of writing, features the message "Gustavo Rosario is a Zeta" imposed over an image of carved jack-o-lanterns.
Following this, two individuals identifying themselves as administrators of the Mexican affiliates of Anonymous distanced themselves from it and all actions related to "Operation Cartel," or "#OpCartel," as it has become known on Twitter. In an October 30 interview with Mexico's Milenio, the individuals claimed to have canceled the operation, citing the risks involved.
Since then, Anonymous Mexico has reversed its stance, claiming on its Facebook page that the operation has been taken up again, although they warn less experienced members to stay away from it. In cooperation with Anonymous Iberoamerica, the largest Spanish-speaking Anonymous network, the group on Monday set up an online form where visitors can report individuals who have connections with the Zetas. In addition to this, a source close to the operation told the New York Times they were in possession of a "list of about 100 or so of the major contacts of the Zetas." Armed with the names and personal details of these individuals, the hacker group seems to have thrown their hat into the ring and taken on the confrontation with their Zeta foes.
On one level, the incident can be interpreted as further proof that a new front in the "drug war" has opened up on the Internet. Increasingly, Mexican drug trafficking organizations have been using the web to threaten rivals, proclaim their innocence and brag about their exploits. Web page comments, YouTube videos and Twitter feeds have all been employed by Mexican cartels to communicate with the public. But as the deaths of the bloggers in Nuevo Laredo illustrate, this virtual battleground can have very real consequences.
On another level, the incident is an illustration of the role that fear plays in the Zetas' exercise of power. Anonymous members' doubts about the operation are well-founded, as the Zetas are generally thought of as the most dangerous drug cartel in Mexico, who carry out brutal public revenge on their enemies. But as the hacking collective decided to go through with the operation, the Zetas could be in a highly vulnerable position. If they give in to Anonymous' demands and free the kidnapping victim — presuming he or she exists — then they risk opening themselves up to further challenges to their authority.
This is especially important to the Zetas, as they don't have the support base that other groups (like the Sinaloa Cartel in the Sierra Madre, or the once-mighty Familia Michoacana in Michoacan) possess. Conversely, if they don't turn over the kidnapping victim, then they risk damaging much of the connections that keep their business together in the Veracruz area.
Thoughts on Hackers vs Drug Gangs in Mexico
El extremo este de la frontera EE. UU.- México: ¿un enclave criminal olvidado?
The US-Mexico Border's Eastern End: A Forgotten Criminal Enclave?
Millions Stolen by Hackers Shows Vulnerability of Mexico's Banks
Los Moreco, Worrying New Type of Criminal Group for Costa Rica


text:
Nickolas "Nick" Latta (* 5. Oktober 1993 in Schongau) ist ein deutsch-kanadischer Eishockeyspieler, der seit Februar 2022 bei den Ravensburg Towerstars in der DEL2 unter Vertrag steht.

Karriere
Nickolas Latta spielte ab der Saison 2008/09 für den SC Riessersee in der Deutschen Nachwuchsliga (DNL). In seiner ersten Spielzeit erzielte der Stürmer in 35 Spielen 10 Tore und insgesamt 17 Punkte. Mit seinem Team schied er in den folgenden Play-offs in der ersten Runde gegen die Juniorenmannschaft der Heilbronner Falken aus. In der DNL-Saison 2009/10 konnte Latta seine Punkteausbeute deutlich steigern und in 34 Partien 31 Tore sowie 31 Torvorlagen erzielen. Der SC Riessersee konnte sich jedoch nicht für die Play-offs qualifizieren.

Nick Latta wurde beim CHL Import Draft 2010 in der zweiten Runde an 62. Position von den Sarnia Sting aus der Ontario Hockey League (OHL) ausgewählt. Er entschied sich für einen Wechsel nach Nordamerika und absolvierte in der OHL-Saison 2010/11 für die Sting 61 Spiele, in denen er 15 Scorerpunkte erzielte. Insgesamt 4 Jahre spielte er für die Stings in der kanadischen Juniorenliga, wobei er im letzten Jahr immerhin 66 Punkte (38 Tore, 28 Assists) erzielen konnte.

Nachdem er mit 20 Jahren die Altersgrenze für die Juniorenliga erreicht hatte, erhielt er 2014 die Möglichkeit für das Farmteam der New York Rangers – den Hartford Wolf Packs – in der AHL zu spielen, wo er in 11 Spielen 2 Punkte (1 Tor, 1 Assist) erzielte. Als ihm für die Saison 2014/15 die Abschiebung in die ECHL zu den Greenville Road Warriors drohte, kehrte er in die Deutsche Eishockey Liga zurück und unterschrieb einen Vertrag bei den Kölner Haien, welcher während der Saison 2014/15 um ein weiteres Jahr verlängert wurde.

Am 10. Januar 2018 kündigte er den Vertrag bei den Kölner Haien. Am 12. Januar 2018 unterschrieb er bei den Wichita Thunder einen Vertrag bis zum Ende der Saison. Anfang April 2018 wurde Latta bei den Grizzlys Wolfsburg als Neuzugang verkündet. Nach zwei Jahren in Wolfsburg (17 Scorerpunkte in 82 Spielen) wechselte er zur Saison 2020/21 zu den Straubing Tigers.

Im Mai 2021 wurde Latta von den Blue Devils Weiden aus der Oberliga Süd verpflichtet und traf dort auf seinen Bruder Louis und seinen Vater Ken, letzterer war bei den Blue Devils als Sportdirektor angestellt. Im Februar 2022 wurde Ken Latta in Weiden freigestellt und seine Söhne verließen den Club. Wenige Tage später wurden die Brüder von den Ravensburg Towerstars aus der DEL2 verpflichtet.

International
Nick Latta vertrat die deutsche Nationalmannschaft erstmals bei einem internationalen Turnier bei der U20-Junioren-Weltmeisterschaft 2011. Der Angreifer absolvierte in diesem Turnier vier Spiele, in denen er ohne Punkterfolg blieb.

Erfolge und Auszeichnungen
 2012 Aufstieg in die Top-Division bei der U20-Junioren-Weltmeisterschaft der Division IA

Karrierestatistik

International

Familie
Sein Vater Ken war ebenfalls professioneller Eishockeyspieler und ist derzeit als Trainer tätig. Sein Onkel David war ebenfalls professioneller Eishockeyspieler.

Weblinks

Einzelnachweise

Eishockeyspieler (Sarnia Sting)
Eishockeyspieler (Hartford Wolf Pack)
Eishockeyspieler (Kölner Haie)
Eishockeyspieler (Wichita Thunder, ECHL)
Eishockeyspieler (Straubing Tigers)
Eishockeyspieler (Grizzlys Wolfsburg)
Eishockeyspieler (EV Ravensburg)
Kanadier
Deutscher
Geboren 1993
Mann


Come see me and my watercolor paintings at the annual MOSAICS Festival for the Arts this coming weekend, September 16-18, on historic Main Street in Downtown St. Charles. Hours are 4 to 9 p.m. Friday evening, 11 a.m. to 9 p.m. Saturday, and 11 a.m. to 5 p.m. Sunday. This is always a fun show in a great setting. All the artists will be on Main Street north of First Capitol.
For a sample of my work, check my web site: www.maggiemccarthy.com, but I will be framing and matting new pieces this week for the MOSAICS show that are not on the web site yet.


Lu Jinnian went to his study room to get a document before returning back down.
Madam Chen saw him coming out of the elevator and immediately stopped what she was doing.
Lu Jinnian nodded, expressionless, and walked towards the shoe cabinet to change his shoes. As he reached for the keys on the cabinet, he turned to look at Madam Chen, who was cleaning an antique porcelain vase. He paused for a few seconds before asking, "How has Mrs. Lu's health been these few days?"
Madam Chen truthfully reported, "Mrs. Lu fully recovered yesterday and her spirits are much higher today. I don't think theres much of an issue..."
Before Madam Chen could finish her sentence, Lu Jinnian had already left with his car keys.
He acted as though it wasn't him who had inquired about Qiao Anhao's condition but rather Madam Chen who had forced the information on him.
Lu Jinnian opened the car door and sat inside. He turned into the empty road at the side and made a turn. When he was looked at the road through the back mirror, he caught sight of Qiao Anhao. She was holding onto a parasol, picking flowers in the garden. A spark brightened Lu Jinnian's eyes and he hit the brakes, stopping the car.
He stared at Qiao Anhao through the back mirror for a really long time before he reached for a cigarette. He lit it up, his actions familiar yet dignified, as he continued to stare unwaveringly at Qiao Anhao.
Only when the cigarette was at its end and burned his fingertips did Lu Jinnian come back to his senses. Still, he remained focused on his back mirror as he casually tossed the cigarette into the ashtray. He lowered the window on his side side. Clenching his lips, he forced himself to look away from the back mirror. Forcefully, he held onto the steering wheel and sped away.
Qiao Anhao picked a huge bouquet of flowers, bringing it into the house happily. She got Madam Chen to fetch an empty vase and put the bouquet in. She then started snipping off the excess leaves until she was satisfied enough to put it on the dinning table.
As Qiao Anhao was washing her hands, Madam Chen seemed to have remembered something. She turned to inform her, "Mrs. Lu, Mr. Lu was back to grab a document just now."
Qiao Anhao paused momentarily before acknowledging her without any emotion. She lowered her head and washed her hands seriously, her originally lifted spirits having dampened once again.


On January 25, 2019, the U.S. Congress passed H.J. Res. 28 to "provide funding to several government agencies through the earlier of February 28, 2019, or the enactment of the applicable appropriations legislation." President Trump signed the bill into law on the same day.
The passage of the resolution ends the partial government shutdown that began when the previous resolution expired on December 21, 2018.


John Campbell was my teacher many lifetimes ago. I recommend his presentation (pdf) on treasury bond risk. He correctly points out that a sovereign, floating a fiat currency, with liabilities denominated in its own currency, cannot default. The sovereign has swapped default risk for inflation risk, and inflation is not default. Sovereign debt has no credit risk, it just has inflation risk, which is why those "triple A" ratings for US Treasuries are as meaningful as triple A ratings were for subprime mortgages. Ratings agencies are no better than they were.
The upshot is that nominal sovereign debt is a good bet against deflation, but a bad bet for stagflation. I'm guessing Campbell recommends TIPs. He was in the late 90s (and it was a bad call then).


text:
Miles and Miles of Reptiles: All About Reptiles (Cat in the Hat's Learning Library) Paperback
The Cat in the Hat travels the globe—in his trusty crocodile car—to explore the world of reptiles: lizards, snakes, turtles, and crocodilians. Along the way, young readers learn the characteristics shared by most reptiles; basic information about each group; quirky, fun facts about individual species; and much, much more. Cool creatures featured include komodo dragons, chameleons, geckos, cobras, leatherback turtles, frilled lizards—a virtual Who's Who of the World's Most Remarkable Reptiles. Young readers will slither in delight!
Tish Rabe is the author of eleven previous Cat in the Hat Learning Library titles. She lives in Greenwich, Connecticut.
Among the many books illustrated by Aristides Ruiz are all the Cat in the Hat Learning Library books. He lives in Newark, New Jersey, and Brooklyn.
Joe Mathieu has illustrated countless children's books.
Categories: 4-5 yrs, 6-8yrs
Be the first to review "Miles and Miles of Reptiles: All About Reptiles (Cat in the Hat's Learning Library) Paperback" Cancel reply
Pop-Up Peekaboo! Playtime Hardcover – Pop up
My First 1000 Words Paperback
Pop-Up Peekaboo! Kitten Board book Hardcover


Filed under Israel and Palestine, israel and palestine articles by Father Dave on Nov 9th, 2013. Comment.
Comments on Israel destroys the Bishop's house!
it seems Israel may have destroyed Bishop's house in retaliation for 2 tweets sent on 5th November from President Rouhani (@Rouhani) to the Pope (@pontifex) in which greetings of Hope Peace & Goodwill were exchanged along with promises to fight violence & terrorism wherever it manifests itself.


Chris Fenwick's Custom Tutorials - Home - A Thousand Words.
Not sure how to classify this piece. I just enjoyed it. I first saw it about a year ago when it was released but back then I wasn't really into this vligity blog MyFace/SpaceBook thing. But I thought I'd share this here so I could find it again later... Anyway, cleaver story telling.
Love the storytelling. It's very clever and the title is perfect. Wish there was more as well! But I like that it leaves you hanging.
"Almost every young people have one or more NBA jerseys. It is not only a way to show the pride for the favorite teams, but also comfortable when you are exercising. Discount NHL jerseys are the best choice for wearing in summers. The authentic jerseys are so expensive that not any average football fan can afford. Then, you can get it online for bargain. "
Christian Louboutin Replica Christian Louboutin Replica.


Columbia Omni Reclining Bath Shower And Commode Transfer System comes reclining feature that provides better positioning and support. The Auto-Safety Stop system prevents chair from accidentally falling off base while bacteria and fungal-resistant ComfortMesh cover ensures clean comfort.
Buy this product and earn 185.03 Reward Dollars.
Seat height range 23.5" to 27.5" 26.5" to 33.5" 23.25" to 27.5"
Overall length (transfer system) 52" 52" 52"
Tub clearance 13-7/8" to 20" 13-7/8" to 20" 13-7/8" to 20"
Are there any precautions to be taken care of?
To reduce the risk of injury or drowning, NEVER leave the user unsupervised or unattended while using this product.
Determine, with a physician or therapist, the suitability of this product for the intended user.
Check regularly that all tubing, bolts, buckles, and other parts are tight at ALL times.
When occupied, make sure the user is buckled in at all times.
How do I clean the fabric cover?
- Adjust the back and calf support frames to horizontal. Turn the seating up- side down and remove velcro strap.
- Slip the cover over the back and calf supports.
Using warm water (100°F/38°C) and household laundry detergent, wash the cover in the washing machine using gentle cycle.
What is the fabric cover made of?
The fabric cover for Omni Transfer Systems is made of polyester that is durable, antimicrobial, resilient, quick drying, fade resistant, and machine washable.
How do I clean the transfer system?
Soapy water or mild cleansers may be used on all parts of your Omni Transfer Systems. Harsh abrasive cleansers may dull the finish.
With the legs in the open and locked positions, place the transfer base into the shower or tub. Then, roll the seating to the end of the tub base. Note: The shuttle base is reversible and can be installed on the slide rails in either direction to accommodate any bathroom layout.
Adjust the leg height of the tub base so the frame tubes are at the same height as the rolling base and both are aligned when positioned end to end.
Make rough adjustments (¾") with the detent buttons, or make fine adjustments by loosening the back knobs and turning the legs to the desired height. Tighten the adjusting knobs when the height is set.
When the heights of the tub base and the rolling base are equal, move the rolling base as close as possible to the tub base. Place the tongue of the manual locking latch over the receiver on the tub base.
Lock the rolling base to the tub base with the center latch before attempting to transfer or slide the rolling base. Loop the tongue from the tub base over the hook receiver on the rolling base. Lock the base to the seating by pulling down on the manual locking handle until the safety lock clicks in place. The safety lock prevents the seating base from rolling away.
Prior to transfer, raise the calf support high enough to clear the sides of the tub.
When transferring, roll the shuttle base until the latch on the back clicks into the position lock bolt. There are position lock bolts on rolling base and tub base. These will lock the seating into a secure position and eliminate any side movement and/or rolling during use. Note: The lock bolt on the tub base can be repositioned into two other locations for better positioning of the individual over the tub in certain applications.
To release the lock, pull upward on the black knob on the lower back of the slider and allow it to travel between the coupled rolling base and bath tub base.


Motorcraft XR Engine Oil 15W-40 with 1 liter capacity for Ford Transit.
These engines hold about 6 liters of oil. This capacity is measured when replacing oil with oil filter.
This is a mineral oil recommended for diesel engines. It can be used with Ford Transit 2.4 Diesel, 2.5 Diesel and 2.5 Turbodiesel engines.


A German official holds his microphone next to his two mobile phones during a meeting of the German federal Parliament in Berlin in February 2014.
Verizon received 148,903 U.S. government requests for customer information in the first half of 2014, slightly less than the 160,733 requests from half of 2013, according to Verizon's second transparency report.
The report lists the number of subpoenas, orders, warrants and emergency requests Verizon received from Jan. 1 to June 30, and are on par to roughly meet by the year's end the 321,545 requests Verizon received in 2013. Arriving amidst heavy debate on NSA surveillance and a NSA reform bill passed by the House in May, the report suggests that law enforcement requests for customer data have remained relatively steady. Verizon notes that the "vast majority of these various types of demands relate to our consumer customers," not enterprise customers.
Verizon for the first time provided specifics about the number of customers affected by government requests: the 72,342 subpoenas received in the first half of 2014 sought data for 132,499 people, for an average of 1.8 people per subpoena.
Orders are broken down into wiretap (accessing content of communication), pen register (phone numbers of outgoing calls), trap & trace (phone numbers of incoming calls) and general (all other orders). While wiretap orders have fallen slightly, all others have increased.
Verizon also reports the law enforcement data demands for customers outside of the United States. Requests in Germany have significantly fallen, a statistic arriving on the heels of the German government terminating a contract with Verizon in June due to fears of U.S. spying. Italy, France and Belgium saw the greatest increases, despite their condemnations of U.S. digital surveillance.
Data on national security demands — which include NSA requests under the Foreign Intelligence Surveillance Act — are largely not reported due to legal restrictions. Verizon disclosed broad ranges, reporting that in 2013, there were 0 to 6,000 national security demands seeking information about 11,000 to 17,000 people.


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Lincoln Parish Sheriff's Office addresses motorists and cyclists safety
After being grazed by several cars in Lincoln Parish, two cyclists are helping to address the issue
LINCOLN PARISH, La. (7/18/19)– If you're a Ruston resident, chances are you've seen Ian Macaskill and Tom Futrell on the road. The men are two of many avid cyclists in Lincoln Parish.
For Macaskill and Futrell, cycling is a part of life, but lately, their love for the sport has put them in danger.
"I've had my elbow hit by mirrors, rear view mirrors; literally bumped as people pass by me," said Futrell.
Futrell says these motorists are passing by at the speed of light, making it a huge safety concern for cyclists.
"If a driver hits a cyclist, and say they're going 25 to 20 miles an hour, the chances of fatality is about 5%, but double that, and it goes up to 65%," said Futrell.
Macaskill believes drivers rushing to their destination is making the issue worse.
"One of the problems is, motorists seem to be impatient, they seem to be in a hurry, and there are certain laws that they don't follow," said Macaskill.
Laws that the Lincoln Parish Sheriff's Office will start heavily enforcing.
"Bicyclists have the same right to the highway as a motorist. They do have duties, they're supposed to ride to the right side of the road and signal before they turn," said Stephen Williams, Public Information Officer with the Lincoln Parish Sheriff's Office.
Williams says drivers need to slow down and give cyclists at least three feet of room. If you want to pass a cyclist, you need to wait until the right of way is clear with no oncoming traffic.
Cyclists also have a responsibility to help drivers.
"Cyclists ought to be predictable, right? If you're going to be riding a bicycle, don't for whatever reason just pull into the middle of the road, you know? You have to do the same things. pay attention to where you are," said Futrell.
Drivers that fail to adhere to these laws could face up to $200 in fines.
by Nancy Cook / Jan 21, 2020
BENTON, La. (KTAL/KMSS) - One of the three people charged in the March shooting death of a Benton man was in Bossier District Court today.
Shawna Jones, 30, is one of three people charged in the death of 29-year-old Caleb Pippenger, who was fatally shot outside his Benton home on the evening of March 15, 2019.