text:
Homologation (Greek homologeo, ὁμολογέω, "to agree") is the granting of approval by an official authority. This may be a court of law, a government department, or an academic or professional body, any of which would normally work from a set of strict rules or standards to determine whether such approval should be given. The word may be considered very roughly synonymous with accreditation, and in fact in French and Spanish[1] may be used with regard to academic degrees (see apostille). Certification is another possible synonym, while to homologate is the infinitive verb form.
In today's marketplace, for instance, products must often be homologated by some public agency to assure that they meet standards for such things as safety and environmental impact. A court action may also sometimes be homologated by a judicial authority before it can proceed, and the term has a precise legal meaning in the judicial codes of some countries.
The equivalent process of testing and certification for conformance to technical standards is usually known as type approval in English-language jurisdictions.
Another usage pertains to the biological sciences, where it may describe the similarities used to assign organisms to the same family or taxon, similarities they have jointly inherited from a common ancestor.
In motorsports a vehicle must be type approved by the sanctioning body to race in a given league, such as World Superbikes, International Level Kart Racing, or other sportscar racing/touring car racing series.
Where a racing class requires that the vehicles raced be production vehicles only slightly adapted for racing, manufacturers typically produce a limited run of such vehicles for public sale so that they can legitimately race them in the class. These vehicles are commonly called "homologation specials".[2]
The term is also applicable in the Olympic Games, in venue certifications, prior to the start of competition. An issue was raised at Cesana Pariol—the bobsleigh, luge, and skeleton track used for the 2006 Winter Olympics in Turin—over its safety in luge. This delayed homologation of the track from January 2005 to October 2005 in order to achieve safe runs during luge competitions.
European professional qualification directives
Homologation reactions that extend an alkyl chain by one methylene (-CH2-) unit
NARIC
Type approval
^ Homologation Specials, www.rallycars.com.
Academic homologation
Education, recognition of diplomas and NARIC in the European Union
Academic homologation in Spain
IWSF Homologation Dossiers—International Waterski & Wakeboard Federation Tournament Waterskiing
ACI Vallelunga Circuit
The Autodromo Vallelunga Piero Taruffi is a racing circuit situated 32 km (20 miles) north of Rome, Italy, near Vallelunga of Campagnano. Vallelunga was built as a sand 1.8 km (1.102 miles) oval in 1959. From 1963 the circuit held the Rome Grand Prix, and in 1967 a new loop was added when the track became the property of the Automobile Club d'Italia (ACI). Further refurbishment was undertaken in 1971. The track is named for the famous Italian racing driver Piero Taruffi.
In August 2004 work started on a 1 km (1,093.6 yards) extension to the track, bringing the track up to its current length. The new configuration has received homologation from the FIA as a test circuit, being used by various Formula One teams. The circuit has also hosted the 6 Hours of Vallelunga endurance event.
The track is also used by ACI for public driving safety training courses, and in autumn of each year hosts a vast flea-market specialising mainly in vintage automotive spare parts.
The circuit is home to simulation software developers, Kunos Simulazioni, who occupy a pit garage as an office.
Arndt–Eistert reaction
The Arndt–Eistert reaction involves a series of chemical reactions that synthesise a carboxylic acid from its homologue with one fewer carbon atoms (i.e. the conversion of RCOOH to RCH2COOH). Named for the German chemists Fritz Arndt (1885–1969) and Bernd Eistert (1902–1978), Arndt–Eistert synthesis is a popular method of producing β-amino acids from α-amino acids. Acid chlorides react with excess diazomethane to give diazoketones. In the presence of a nucleophile (water) and a metal catalyst (Ag2O), diazoketones will form the desired acid homologue.
While the classic Arndt–Eistert synthesis uses thionyl chloride to prepare the acid chloride intermediate, alternative procedures can be used to effect this transformation. The diazoketone is traditionally generated using diazomethane, but other methods such as diazo-group transfer can also be applied. Diazomethane is toxic and violently explosive, which has led to safer alternative procedures being developed, such as the usage of ynolates (Kowalski ester homologation) or diazo(trimethylsilyl)methane.
Autodromo di Franciacorta
Autodromo di Franciacorta is a race track located in the homonymous area of Franciacorta from which it takes its name, in Castrezzato in the province of Brescia. The racetrack has received homologation from the FIA for motor racing competitions and from the FMI for motorcycling ones. The circuit was inaugurated in 2006.
Diesel 2000 is an FIA circuit racing classification for modified production based touring cars using turbodiesel engines.
Like its counterpart, Super 2000, the category is open to large-scale series production touring cars modified by a kit. Cars must have at least four seats and at least 2500 fully identical units must be produced within 12 consecutive months to allow homologation. However, unlike Super 2000, Diesel 2000 allows only 4-cylinder turbocharged diesel engines with a maximum capacity of 2000cc.The category was introduced to the European Touring Car Championship for 2004 to allow turbodiesel cars to compete alongside the existing petrol engined Super 2000 vehicles.
When the European Championship was upgraded to become the World Touring Car Championship in 2005, both Diesel 2000 and Super 2000 cars were eligible to compete for the new title.Spanish manufacturer SEAT has won the manufacturers award of the World Championship in both 2008 and 2009 with their Diesel 2000 León TDI model. Factory SEAT drivers Yvan Muller and Gabriele Tarquini have won the drivers titles with the same model in these two years respectively.
The Ferrari GTO (often referred to as Ferrari 288 GTO)(Type F114) is an exotic homologation of the Ferrari 308 GTB produced from 1984 to 1987 in Ferrari's Maranello factory, designated GT for Gran Turismo and O for Omologata (homologated in Italian).
Ford Escort RS Cosworth
The Ford Escort RS Cosworth is a sports derivative and the 1st 2500 were rally homologation special of the fifth generation European Ford Escort. It was designed to qualify as a Group A car for the World Rally Championship, in which it competed between 1993 and 1998. It was available as a road car from 1992–1996 in very limited numbers. The smaller turbo cars were not F.I.A recognised and only the first 2500 cars made before 1 January 1993 are in fact "Homologation special versions." It was instantly recognisable due to its large "whale tail" rear spoiler. The main selling point was the Cosworth YBT, a highly tunable turbocharged 2.0 L (1,993 cc) with a bore x stroke of 90.8 mm × 77 mm (3.57 in × 3.03 in) Inline-four engine which had an output of 227 PS (167 kW; 224 bhp) in standard trim. Tuning companies have achieved power outputs of over 1,000 bhp (746 kW; 1,014 PS).
Ford RS200
The Ford RS200 is a mid-engined, four-wheel drive sports car that was produced by Ford Motorsport in Boreham, UK, from 1984 to 1986. The road-going RS200 was the basis for Ford's Group B rally car and was designed to comply with FIA homologation regulations, which required 200 parts kits to be produced and at least one road-legal car to be assembled. It was first displayed to the public at the Belfast Motor Show.
Group 2 (racing)
The Group 2 racing class referred to regulations for cars in touring car racing and rallying, as regulated by the FIA. Group 2 was replaced by Group A in 1982.
The FIA established Appendix J regulations for Touring and GT cars for 1954 and the term Group 2 was in use to define Touring Cars in the Appendix J of 1959. By 1961 Appendix J included specifications for both Group 1 Series Touring Cars and Group 2 Improved Touring Cars with a minimum production of 1,000 units in twelve consecutive months required to allow homologation of a model into either group. Technical modifications beyond those allowed for Group 1 cars were permitted in Group 2.The British Saloon Car Championship was open to Group 2 cars each year from 1961 to 1965 and from 1970 to 1973.Group 2 was the specified category for the European Touring Car Challenge from 1963 to 1967 and the cars were also eligible alongside Group 5 special touring cars in 1968 and 1969. It was again the premier category when the series was renamed as the European Touring Car Championship for 1970 and continued to be so until it was replaced by Group A for 1982.The Sports Car Club of America's Trans-American Sedan Championship was contested by Group 2 touring cars from its inception in 1966 through to the 1972 season.
Group A was a set of motorsport regulations introduced by FIA covering production-derived vehicles intended for outright competition in Touring car racing and Rallying. In contrast to the short-lived Group B and Group C, the Group A referred to production-derived vehicles limited in terms of power, weight, allowed technology and overall cost. Group A was aimed at ensuring a large number of privately owned entries in races.
Group A was introduced by the FIA in 1982 to replace the outgoing Group 2 as "modified touring cars", while Group N would replace Group 1 as "standard touring cars". The FIA continued to promulgate regulations for Group A Touring Cars until at least 1993, and the category survived in domestic championships until 1994. However, Group A is still used as the basis for most rally competitions around the world.
Group GT1 also known simply as GT1, was a set of regulations maintained formerly by the Fédération Internationale de l'Automobile, for Grand Tourer racing. The category was first created in 1994, as the top class of the BPR Global GT Series, and was included in the 24 Hours of Le Mans. It fell under FIA regulation from 1997, after the BPR series came under the control of the FIA, becoming known as the FIA GT Championship. The category was dissolved at the end of 2011. The category may be split into 4 distinctive eras, from its debut in 1994-1996,1997-1998, 2000-2009, 2010-2011.
Group GT3, known technically as Cup Grand Touring Cars and commonly referred to as simply GT3, is a set of regulations maintained by the Fédération Internationale de l'Automobile (FIA) for grand tourer racing cars designed for use in various auto racing series throughout the world. The GT3 category was initially created in 2005 by the SRO Group as a third rung in the ladder of grand touring motorsport, below the Group GT1 and Group GT2 categories which were utilized in the SRO's FIA GT Championship, and launched its own series in 2006, the FIA GT3 European Championship. Since then, Group GT3 has expanded to become the de facto category for many national and international grand touring series, although some series modify the ruleset from the FIA standard. By 2013, nearly 20 automobile manufacturers have built or been represented with GT3 machines.
Group GT3 allows for a wide variety of car types to be homologated with almost no limit on engine sizes and configurations or chassis construction or layout. GT3 cars must be based on production road car models in mass production. Performance of all the Group GT3 cars are regulated, either by the GT Bureau of the FIA or by a series' specific ruling body, through Balance of Performance formulae that adjusts limits on horsepower, weight, engine management, and aerodynamics to prevent a single manufacturer from becoming dominant in the class. The cars in GT3 are designed to have a weight between 1200kg and 1300kg (2645lbs and 2866lbs) with horsepower between 500hp and 600hp. All cars have a very similar power to weight ratio but achieved either by high power and high weight such as the Mercedes-Benz SLS AMG or low power and low weight such as the Porsche 911 GT3. GT3 cars also have traction control, ABS and built in air jacks for quick pit stops.
Group R-GT
Group R-GT (or sometimes Group RGT), is a FIA specification for GT cars in rallying. The R-GT regulations were introduced in 2011, and since 2014 technical passports for individual vehicles can be obtained. Thus a homologation for specific car models is no longer required.Internationally, R-GT cars compete in the FIA R-GT Cup, which is contested on tarmac rounds of the ERC and WRC.
Homologation (motorsport)
In motorsports, homologation is the type approval process through which a vehicle, a race track, or a standardised part is required to go for certification to race in a given league or series. The process of testing and certification for conformance to technical standards is usually known as type approval in English-language jurisdictions. The regulations and rules that must be met are generally set by the series' sanctioning body. The word is derived from the Greek homologeo—literally "I say the same"—for "agree".
Homologation reaction
A homologation reaction, also known as homologization, is any chemical reaction that converts the reactant into the next member of the homologous series. A homologous series is a group of compounds that differ by a constant unit, generally a (-CH2-) group. The reactants undergo a homologation when the number of a repeated structural unit in the molecules is increased. The most common homologation reactions increase the number of methylene (-CH2-) units in saturated chain within the molecule. For example, the reaction of aldehydes or ketones with diazomethane or methoxymethylenetriphenylphosphine to give the next homologue in the series.
Examples of homologation reactions include:
Kiliani-Fischer synthesis, where an aldose molecule is elongated through a three-step process consisting of:
Nucleophillic addition of cyanide to the carbonyl to form a cyanohydrin
Hydrolysis to form a lactone
Reduction to form the homologous aldose
Wittig reaction of an aldehyde with methoxymethylenetriphenylphosphine, which produces a homologous aldehyde.
Arndt–Eistert reaction is a series of chemical reactions designed to convert a carboxylic acid to a higher carboxylic acid homologue (i.e. contains one additional carbon atom)
Kowalski ester homologation, an alternative to the Arndt-Eistert synthesis. Has been used to convert β-amino esters from α-amino esters through an ynolate intermediate.
Seyferth–Gilbert homologation in which an aldehyde is converted to a terminal alkyne and then hydrolyzed back to an aldehyde.Some reactions increase the chain length by more than one unit. For example, the following are considered two-carbon homologation reactions.
Kowalski ester homologation
The Kowalski ester homologation is a chemical reaction for the homologation of esters.
This reaction was designed as a safer alternative to the Arndt–Eistert synthesis, avoiding the need for diazomethane. The Kowalski reaction is named after its inventor, Conrad J. Kowalski.
Seyferth–Gilbert homologation
The Seyferth–Gilbert homologation is a chemical reaction of an aryl ketone 1 (or aldehyde) with dimethyl (diazomethyl)phosphonate 2 and potassium tert-butoxide to give substituted alkynes 3. Dimethyl (diazomethyl)phosphonate 2 is often called the Seyferth–Gilbert reagent.
This reaction is called a homologation because the product has exactly one additional carbon more than the starting material.
The Wittig reaction or Wittig olefination is a chemical reaction of an aldehyde or ketone with a triphenyl phosphonium ylide (often called a Wittig reagent) to give an alkene and triphenylphosphine oxide.
The Wittig reaction was discovered in 1954 by Georg Wittig, for which he was awarded the Nobel Prize in Chemistry in 1979. It is widely used in organic synthesis for the preparation of alkenes. It should not be confused with the Wittig rearrangement.
Wittig reactions are most commonly used to couple aldehydes and ketones to singly-substituted triphenylphosphonium ylides. For the reaction with aldehydes, the double bond geometry is readily predicted based on the nature of the ylide. With unstabilised ylides (R3 = alkyl) this results in (Z)-alkene product with moderate to high selectivity. With stabilized ylides (R3 = ester or ketone), the (E)-alkene is formed with high selectivity. The (E)/(Z) selectivity is often poor with semistabilized ylides (R3 = aryl).To obtain the (E)-alkene for unstabilized ylides, the Schlosser modification of the Wittig reaction can be used. Alternatively, the Julia olefination and its variants also provide the (E)-alkene selectively. Ordinarily, the Horner-Wadsworth-Emmons reaction provides the (E)-enoate (α,β-unsaturated ester), just as the Wittig reaction does. To obtain the (Z)-enoate, the Still-Gennari modification of the Horner-Wadsworth-Emmons reaction can be used.
The Yamaha YZF750 is a motorcycle that was produced from 1993 to 1998 in two forms, the standard R and the homologation model single seat SP. The 750R was the only version sold in the US.
Mechanically the later SP differed from the R in the following areas: adjustable swingarm pivot position, 39 mm Keihin FCR flatslide carburetors, a lower screen, a removable rear subframe and a single seat. The primary drive, gear box and final drive ratios are different on the SP. The rear suspension unit is different and vastly improved for the earlier SP however the R from 1996 also had the Ohlins rear shock. The SP was the homologation model of the Yamaha YZF750 for the World Superbike Championship before the rules changed to allow 1000cc bikes. The bike won the Suzuka 8 Hours endurance race four times between 1987 and 1996.


text:
\section{Introduction}

Recent first direct detections of gravitational waves with the two LIGO
detectors \cite{GW150914,GW151226} create an unprecedented opportunity for
studying the Universe through a novel, never before explored channel of
spacetime fluctuations. Advanced LIGO \cite{ALIGO2015} and Advanced Virgo
\cite{AdV2015}, few-kilometer long arm laser interferometric detectors are
sensitive in the range of frequencies between 10 Hz and a few kHz.  They
registers a coherent signal emitted by a bulk movement of large, rapidly-moving
masses. Once emitted, gravitational waves are weakly coupled to the surrounding
matter and propagate freely without scattering. This has to be contrasted with
the electromagnetic emission which originates at the microscopic level, is
strongly coupled to the surroundings and often reprocessed; it carries a
reliable information from the last scattering surface only. Gravitational wave
observations are therefore the perfect counterpart to the electromagnetic
observations as they may provide us with information impossible to obtain by
other means.

In addition to inspiralling and merging binary systems, among promising
sources of gravitational radiation are all asymmetric collapses
and explosions e.g., supernov{\ae}. wide binary systems, rotating deformed
stars (gravitational-wave `pulsars' of continuous and transient nature), as
well as stochastic background waves produced by whole populations of sources.

In the following we will briefly describe astrophysical motivation behind
continuous gravitational waves produced by rotating deformed neutron stars
(Sect.~\ref{sect:motiv}), data-analysis methods and computational challenges
related to them (Sect.~\ref{sect:meth}), Advanced LIGO O1 run results
(Sect.~\ref{sect:curr}), and plans for the future (Sect.~\ref{sect:plans}).

\section{Astrophysical motivation} \label{sect:motiv}

Neutron stars are the most relativistic, dense and compact {\em material}
objects in the Universe.  Their compactness i.e., mass-to-radius ratio
$2GM/Rc^2$ reaches 0.5 ($G$ being the Newton's constant, $c$ the speed of
light); for comparison, the compactness of the most compact objects, black
holes, equals 1. Their average density surpasses the nuclear saturation density
i.e., the density of atomic nuclei.  At these densities matter exists most
probably in an `exotic' phase, e.g., as de-confined quarks. Neutron stars are
self-gravitating objects stabilized by strong force interactions, gigantic
nuclei of masses up to $2\,M_\odot$, radii about $10-15$ km with surface
magnetic fields of $10^8-10^{15}$ Gauss, that can spin several hundred times
per second. Comparison of realistic models of neutron stars with a variety of
astrophysical observations - including the gravitational waves they emit - is
the only way to peek into a realm of dense matter strong interactions much
above the nuclear saturation density.

Neutron stars provide truly unique conditions to study matter at the most
extreme densities, pressures, and in the presence of powerful magnetic fields.
These conditions cannot be reproduced (or even approximated) in terrestrial
laboratories. At present, about 2500 neutron stars are known, and an estimated
number of $10^8-10^9$ exists in every galaxy similar to ours. Neutron stars
play an important role in many astrophysical phenomena: they are observed in
all the EM spectrum as radio-, X- and $\gamma$-pulsars, magnetars, are present
in supernov{\ae} remnants, in many accreting systems and in relativistic double
neutron star binaries, yet very little is known about their internal
composition. What is conventionally accepted is that at least some part of
neutron-star interior - the outer part about 1 km thick called the crust,
corresponding to densities {\em below} the nuclear saturation density - is in
the crystalline state.

In the following we will focus on rotating, non-axisymmetric neutron stars as
sources of continuous periodic gravitational wave emission. Continuous
gravitational wave is by definition a long-lived phenomenon, $T > T_{obs}$, and
its frequency $f_{GW}$ is somehow proportional to the spin frequency of the star $f$,
$f_{GW}\propto f$. There are several proposed astrophysical mechanisms
providing the necessary asymmetry, which in the case of a rotating star is the
source of time-varying quadrupole required for the gravitational-wave emission.
Mechanisms include neutron-star ''mountains'', supported by elastic and/or
magnetic stresses ($f_{GW} = 2f$), oscillations (e.g., r-modes
\cite{AnderssonK2001}, $f_{GW} = 4/3f$), free precession ($f_{GW}\propto
f + f_{prec}$) and accretion that drives the deformation from r-modes,
thermal gradients and magnetic fields ($f_{GW}\simeq f$). For a recent
review see \cite{Lasky2015}.

The most-commonly used and the simplest model of the non-axisymmetric rotating
neutron star radiating purely quadrupolar waves consists of a triaxial
ellipsoid (with moments of inertia along the axes $I_1$, $I_2$, $I_3$),
rotating about one of the principal directions of its moment of inertia tensor
($I_3$, say). Such a body radiates GWs at the frequency twice the rotational
frequency of the star, $2\pi f_{GW} = \Omega_{GW} = 2\Omega$. The strain signal
at the detector changes in time as
\begin{equation}
h(t) = h_0\left( \frac{1}{2}F_+(t,\alpha,\delta,\psi)\left(1+\cos^2\iota\right)\cos(\phi(t) + \phi_0)
+ F_\times(t,\alpha,\delta,\psi)\cos\iota\cos(\phi(t) + \phi_0)\right),
\label{eq:triaxial}
\end{equation}
where $h_0$ is the gravitational-wave strain amplitude, $\alpha$ and $\delta$
are right ascension and declination of the source in the sky, $\psi$ is the
polarization angle, and $\iota$ the inclination of the rotation axis to the
line of sight. Phase of the signal $\phi(t) + \phi_0$ incorporates the possible
evolution of the spin frequency. $F_+$ and $F_\times$ are the antenna responses
of the detector, corresponding to two gravitational-wave polarizations $+$ and
$\times$.

From the quadrupole formula \cite{Einstein1918}, amplitude $h_0$ is estimated as follows:
\begin{eqnarray}
h_0 = \frac{16\pi^2G}{c^4}\frac{I\epsilon f^2}{d} =
4\times 10^{-25}\left(\frac{\epsilon}{10^{-6}}\right)
\left(\frac{I}{10^{45}\ {\rm g\ cm^2}}\right)
\left(\frac{f}{100\ {\rm Hz}}\right)^2
\left(\frac{100\ {\rm pc}}{d}\right),
\label{eq:h0}
\end{eqnarray}
where $I\equiv I_3$, $f=\Omega/2\pi$, $\epsilon = (I_1 - I_2)/I$ is is the
fiducial equatorial ellipticity of the star (a ''deformation''), and $d$ is
typical distance in the Galaxy.  According to theoretical studies of the dense
matter equation of state \cite{J-MO2012,Owen2005,UCB2000}, nucleonic matter may
sustain deformations up to $\epsilon \simeq 10^{-6} - 10^{-7}$, whereas for
quark matter $\epsilon$ can reach $10^{-4} - 10^{-5}$.

Observations of the majority of known pulsars show that their spin frequency
slowly decreases, $\dot{f} < 0$ (exceptions are pulsars in binary systems which
can be spun-up by the angular momentum transfer from the accretion disk). A
useful quantity related to the amount of kinetic (rotational) energy of the
star is the so-called spin-down limit. It is derived by assuming that the
gravitational-wave emission alone is responsible for the change in the
rotational energy, $\dot{E}_{\rm rot}$. For $E_{\rm rot} = 2\pi^2If^2$,
$\dot{E}_{\rm rot}\propto If\dot{f\ }$ is equated with the GW emission,
$\dot{E}_{\rm GW}\propto \epsilon^2 I^2 f^6$ to obtain the spin-down limit
amplitude
\begin{eqnarray}
h_{\rm sd} = \frac{1}{d}\sqrt{\frac{5GI}{2c^3}\frac{|\dot{f\ }|}{f}} =
8\times 10^{-24} \sqrt{\left(\frac{I}{10^{45}\ {\rm g\ cm^2}}\right)
\left(\frac{|\dot{f\ }|}{10^{-10}\ {\rm Hz/s}}\right)
\left(\frac{100\ {\rm Hz}}{f}\right)}
\left(\frac{100\ {\rm pc}}{d}\right).
\label{eq:h0sd}
\end{eqnarray}
Comparison with Eq.~\ref{eq:h0} results in the limiting deformation $\epsilon_{\rm sd}$:
\begin{equation}
\epsilon_{\rm sd} = 2\times 10^{-5}
\sqrt{\left(\frac{10^{45}\ {\rm g\ cm^2}}{I}\right)
\left(\frac{100\ {\rm Hz}}{f}\right)^5
\left(\frac{|\dot{f\ }|}{10^{-10}\ {\rm Hz/s}}\right)}
= 0.2\left(\frac{h_{\rm sd}}{10^{-24}}\right)f^{-2}I_{45}^{-1}d_{kpc}.
\end{equation}

A star with $\epsilon_{\rm sd}$ would spin-down solely by gravitational-wave
radiation.  In reality, the ellipticity is smaller, so the results `beating the
spin-down limit' probe the physically interesting range of ellipticities and
set the upper limit for the ellipticity given object has. We will come back to
the spin-down limit in Sect.~\ref{sect:curr}.

\begin{figure}[h]
\begin{minipage}{0.5\linewidth}
\centerline{\includegraphics[width=\linewidth]{figures/data.pdf}}
\end{minipage}
\hfill
\begin{minipage}{0.5\linewidth}
\centerline{\includegraphics[width=\linewidth]{figures/fft.pdf}}
\end{minipage}
\caption{Periodic signal hidden in white Gaussian noise (left), and the
Fourier transform of this time series (right).}
\label{fig:fft}
\end{figure}

\section{Data-analysis methods and computational challenges} \label{sect:meth}

Searching for long-lived, weak gravitational wave signals is a particularly
cumbersome task, especially when nothing is known about its parameters.
Eq.~\ref{eq:h0} shows that their strain amplitude is much smaller than than
e.g., the characteristic strain amplitude of O1 detections, $h\simeq 10^{-21}$.
Fortunately, one may search for weak signals hidden deeply in the noise
provided a waveform of the signal is known. The idea of such a search would be
to compute the cross correlation between the data and a parametrised template
waveform in order to find parameters of the best match. Techniques of this sort
are called the matched filtering methods \cite{Wiener1949,Helstrom1968,Schutz1999}.
Matched filtering provide an optimal detection statistic (it maximizes the signal-to-noise ratio)
if noise is Gaussian.

\subsection{Example: signal-to-noise ratio for a periodic signal}

An instance of a strictly periodic signal ''buried'' in the stationary white
Gaussian noise is presented in Fig.~\ref{fig:fft}. We will estimate the
signal-to-noise ratio $\rho$ by approximating the output of the matched filter,
which in the case of a periodic signal is simply the Fourier transform. The
scalar product $(x\lvert y)$ is defined using the Fourier transform as
\begin{equation}
(x\lvert y) = 4\Re\int_{0}^{\infty}\frac{\tilde{x}(f)\tilde{y}^\ast(f)}{S_n(f)} \mathrm{e}^{2\pi ift} df,
\end{equation}
where $*$ denotes complex conjugation, $\Re$ is the real part of the
integral, and $\tilde{x}(f)$ and $\tilde{y}(f)$ are the Fourier transform of
the time-domain data series:
\begin{equation}
  \tilde{x}(f) = \int_{-\infty}^\infty x(t) \mathrm{e}^{-2\pi ift} dt,
\quad \text{with the inverse transform}\quad
  x(t) = \int_{-\infty}^\infty \tilde{x}(f) \mathrm{e}^{2\pi ift} df.
\end{equation}
$S_n(f)$ is the one-sided power spectral density of the detector's noise. For a
stable detector we may assume the that $S_n(f)\approx S_0=const.$ over the data
span. From the Parseval theorem,
\begin{equation}
  \left(x\lvert y\right) \approx \frac{2}{S_0}\int_0^T x(t) y(t) dt.
\end{equation}
For the additive noise process, the data $s(t)$ is defined as the sum of the
signal and the noise: $s(t) = h(t) + n(t).$ The matched filter output of the
data stream $s(t)$ with a filter template $h_{templ.}(t)$ (correlation of the
data containing a possible signal with its model) is
\begin{equation}
  4\Re\int_{0}^{\infty}\frac{\tilde{s}(f)\tilde{h}^\ast_{templ.}(f)}{S_n(f)} \mathrm{e}^{2\pi ift} df.
\end{equation}
The optimal signal-to-noise ratio is defined as $\rho := \sqrt{(h\lvert h)}$.
For a periodic signal $h(t) = h_0\cos(\phi(t) + \phi_0)$, we will assume that
the data span $T_0$ is much longer than the period of the wave, $P_0 = 1/f_0$,
and that the phase can be expanded in the series $\phi(t)=\Sigma_{k} a_k
t^{k+1}$. Also
\begin{equation}
  \frac{1}{T_0}\int_0^{T_0} \cos(n\phi(t))dt \approx \frac{1}{T_0}\int_0^{T_0} \sin(n\phi(t))dt \approx 0
\end{equation}
for integers $n>0$. Integrating the $\rho^2$ for $h(t) = h_0\cos(\phi(t) + \phi_0)$ gives the
estimate for the optimal signal-to-noise ratio for a periodic signal of the amplitude $h_0$
\begin{equation}
  \rho = \left(\frac{2}{S_0}\int_0^{T_0} \left(h(t)\right)^2 dt\right)^{1/2}
  \left( \frac{2}{S_0}\int_0^{T_0} h_0^2\cos^2(\phi(t) + \phi_0) dt\right)^{1/2}
  \approx\ h_0 \left(\frac{T_0}{S_0}\right)^{1/2}.
\end{equation}
It is clear that even for a small $h_0$ one can reach a satisfactory signal-to-noise ratio
with a sufficiently long stretch of data.

In practice, on top of the secular spin-down modulation mentioned before (to describe
this feature, one says that the signal is {\em almost monochromatic}), the signal
is modulated by the movement of the detector with respect to the source. Since
the Advanced LIGO and Advanced Virgo detectors are placed on Earth, the
presence of other planets and Earth's rotation influences signal's amplitude
and phase. Demodulation to a frame connected with the Solar System Barycenter
(the place in the Solar System that moves the least with respect to the source),
precise ephemerides of the movement of planets are used. The fact that the
detectors are moving with respect to the source isn't necessary a bad thing,
though: detector movement distinguishes a real signal from local spectral
artifacts, called the ''stationary lines''.

\subsection{Example: the ${\mathcal{F}}$-statistic}

A conceptually relatively simple method to develop a detection statistic using
the time-domain data $s(t)$ is the ${\mathcal{F}}$-statistic
\cite{JaranowskiKS1998}. For a triaxial rotating neutron star model
(Eq.~\ref{eq:triaxial}, the statistic is obtained by maximizing the likelihood
ratio function with respect to the four unknown parameters: $h_0$, $\phi_0$,
$\iota$, and $\psi$. This leaves, in case when only first derivative of $f$
is taken into account, a function of four parameters: $f$, $\dot{f}$, $\alpha$
and $ \delta$. These four parameters form a parameter space in which the
signal's best match will be searched for. Assuming that the observation time
$T_0$ is the integer multiple of sidereal days, and that the bandwidth is
narrow (so that the spectral density of the noise $S_0$ is constant), the
${\mathcal{F}}$-statistic is evaluated \cite{Astone2010p5} as
\begin{equation}
  {\cal F} = \frac{2}{S_0 T_0}\left(\frac{|F_a|^2}{\langle a^2\rangle} +
  \frac{|F_b|^2}{\langle b^2\rangle}\right),
\label{eq:fstat}
\end{equation}
with
\begin{equation}
  F_a = \int_0^{T_0} s(t) a(t) \exp(-i \phi(t)) dt,\quad F_b = \dots,\quad
  \langle a^2\rangle = \int_0^{T_0} a(t)^2 dt,\quad \langle b^2\rangle = \dots,
\end{equation}
$F_a$ and $F_b$ being the generalizations of the Fourier transforms from the
previous section. Amplitude modulation functions $a(t)$ and $b(t)$ are related
to detector's antenna response ($F_+ = a(t)\cos 2\psi + b(t)\sin 2\psi$,
$F_\times = -a(t)\sin 2\psi + b(t)\cos 2\psi$) and depend on the sources' sky
position $\alpha$ and $\delta$, and the phase modulation function $\phi(t)$
depends also on the frequency $f$ and spin-down of the source,
$\dot{f}$. The signal-to-noise ratio $\rho$ is related to $\mathcal{F}$ as follows:
$\rho = \sqrt{2({\cal F} - 2)}$.

\subsection{Taxonomy of search methods}

Continuous gravitational-wave searches can by divided according to the amount
of information one has about the sources.

The {\em targeted searches} are most
often based on matched filtering (data of length $T_0$ correlated with signal
templates). Position, $f$ and $\dot{f}$, sometimes also the source's
orientation are known. In this case the expected strain amplitude scales like
$h_0 \propto \sqrt{S/T_0}$, where $S$ is the amplitude spectral density at the
expected gravitational-wave frequency.

{\em Directed searches} cover the intermediate cases when only some parameters
are known, e.g., the position of the source. Astrophysically, they may be
relevant to supernov{\ae} remnants, the Galactic center, globular clusters,
accreting neutron stars in binary systems (e.g., the brightest X-ray source in the sky,
Sco X-1).

{\em All-sky searches} are the most demanding types of searches. Source
parameters and positions are not known, which makes the parameter space large
and the problem becomes very quickly computationally bound. In order to mediate
this, hierarchical approaches are being used. Instead of analyzing the whole
$T_0$ data span at once, the data is divided into $N$ data segments of length
$T_s$, which are analyzed coherently, and the resulting information is combined
incoherently. The expected strain amplitude scales like $h_0 \propto
\sqrt{S/T_s}/N^{1/4}$. The most sophisticated example of the hierarchical
approach is the volunteer-driven Einstein@Home project \footnote{{\tt
https://einsteinathome.org}}.

\subsection{Example: computational cost for an all-sky search}

In order to optimally cover the $(f, \dot{f}, \alpha, \delta)$ parameter space
of an all-sky search at all possible frequencies, a grid of parameters is
obtained as a solution to the covering problem with constraints (a constraint
being e.g., a condition that the optimal $(\dot{f}, \alpha, \delta)$ lattice
coincides with points in $f$ corresponding to the Fourier frequencies bins of
the Fast Fourier Transform algorithm). Typically, the number of points in $\dot{f},
\alpha, \delta$ scales with some positive power of $T_0$, so, depending
on the details of the implementation \cite{Wette2014}, the computational demand scales like
\begin{equation}
\underbrace{T^2_0}_{\dot{f}}\times\underbrace{T^{[0-3]}_0}_{\alpha,\delta}\times \underbrace{T_0\log(T_0)}_{f\ \text{by FFT}} = T_0^{[3-6]}\log(T_0),
\end{equation}
which is very prohibitive for large $T_0$. A coherent search of $T_0\simeq
1\,yr$ of data (comparable with ongoing and planned Advanced LIGO/Virgo runs)
in the broad sensitivity band of the detectors (10 - 2000 Hz) requires {\em
zettaFLOPS} ($10^{21}$ FLOPS) scale supercomputers. The solution is a
hierarchical scheme: divide the data $T_0$ into a number $N$ shorter length
$T_s$, $T_s\simeq$ days, data segments and perform a coherent search in each of
them (search in narrow frequency bands of bandwidth $B$, Nyquist sampling time
$\delta t = 1/2B$, number of data points $N_p = T_s /\delta t = 2T_s B$).
\begin{figure}[h]
\begin{minipage}{\linewidth}
\centerline{\includegraphics[width=0.4\linewidth]{figures/time_frequency.pdf}}
\end{minipage}
\caption{Division of the time-frequency data into narrow frequency bands of bandwidth $B$,
reference frequency $f_i$, and $N$ time segments of length $T_s$ ($NT_s = T_0$). Each
time-frequency segment is then analyzed separately, allowing for effective parallelization.}
\label{fig:time_freq}
\end{figure}
This is feasible on a typical petaFLOP scale supercomputer (cluster), yet still
requires millions of CPU-hours. Second incoherent stage consists of searching
for coincidences between different $T_s$ segments. Surviving outliers present
in sufficiently many segments (candidate signals with relatively
well-determined parameters) are subjected to a final scrutinizing follow-up (a
''targeted search'').

\section{Continuous gravitational waves in the Advanced LIGO O1 era} \label{sect:curr}

The first Advanced LIGO observing run (O1) started on September 11, 2015 and
finished January 19, 2016. During that time the Hanford and Livingston
detectors collected 78 days and 66 days of science data, respectively.

First published result pertains to a targeted search for gravitational waves
from 200 known pulsars \cite{Abbott2017a}. In this list, 11 high-value target
pulsars, for which the spin-down limit based on Eq.~\ref{eq:h0sd} could either
be improved or closely approached, were identified. These selected pulsars were
analyzed by three, largely independent methods: two time-domain-based methods,
Bayesian \cite{DupuisW2005} and $\mathcal{F}$/$\mathcal{G}$-statistic
\cite{JaranowskiK2010}, and the frequency-domain-based 5n-vector method
\cite{Astone2010,Astone2012}. The remaining 189 targets were analyzed using the
Bayesian method only. The analysis didn't find significant evidence for a
gravitational-wave signal from any of these pulsars, but the most constraining
upper limits to date on their gravitational-wave amplitudes and ellipticities
were obtained. For eight of the high-value target pulsars, new upper limits
give improved bounds over the indirect spin-down limit values. For the Crab
pulsar, the 95\% confidence upper limit for the gravitational-wave radiation
energy is $2\times 10^{-3}\ \dot{E}_{rot}$, and in case of the Vela pulsar, the
upper limit is $10^{-2}\ \dot{E}_{rot}$. The limits on ellipticity correspond
to the relative deformation (the ''mountain'') no greater than $\simeq 10$ cm
and $\simeq 50$ cm for the Crab and Vela pulsars, respectively. For
another 32, values within a factor of 10 of the spin-down limit were found: it
is likely that some of these will be reachable in future runs of Advanced LIGO
and Advanced Virgo. The smallest upper limit was obtained for PSR J1918-0642:
$h_0 = 1.6\times 10^{-26}$. These new results improve on previous limits of
Initial LIGO/Virgo by more than a factor of two (see the summary Fig. 1 of
\cite{Abbott2017a}, where the comparison with the sensitivity curve, initial
detector results and the spin-down limits is presented).

Second publication (in the time of writing available as a preprint) is related
to a directed search for gravitational waves from a bright X-ray source Sco X-1
\cite{Abbott2017b}. Sco X-1 is the brightest Low Mass X-ray Binary (LMXB, a
binary system consisting of a neutron star or a black hole, and a normal star
with lower mass) in the Galaxy. The X-ray radiation is produced during
accretion; neutron stars in these systems are potential sources of continuous
gravitational waves because accretion provides a natural method of building a
deformation on the star and powering the gravitational-wave emission. There are
however challenges in searching for gravitational waves from this particular
source. First, the spin frequency of the neutron star is unknown - the search
has to cover a broad range of frequencies, which means it requires much more
computing power than a directed search in case of a known pulsar. Most likely
the spin frequency is not constant, and not even behaving
strictly monotonously, but ''wandering'' i.e., it changes because of the
fluctuations in the amount of accreted matter; frequency is also modulated by
the orbital motion of the binary system (the signal power is distributed into
sidebands i.e., frequencies higher or lower than the gravitational-wave signal
frequency). In order to perform an efficient search in these circumstances, a
hidden Markov model (a statistical model in which it is assumed that the system
is a Markov process with unobserved states, see \cite{Baum1972} and references
therein and tutorial \cite{Rabiner1989}) was implemented. The search covered a
band of frequencies from 60 Hz to 650 Hz. No detection was claimed from this
search, but very sensitive upper limits on the gravitational-wave strain were
placed (to quote one example: 95\% upper limits $h_0 = 3\times 10^{-25}$ at 100 Hz,
assuming circular polarization).

We also report on an all-sky search for periodic gravitational waves
using the Advanced LIGO's O1 run \cite{O1CWAllSky}, in the frequency band of 20-475\,Hz and a
frequency time derivative range of $[-1.0, +0.1]\times 10^{-8}$\,Hz/s. Several
different data-analysis pipelines took part in this study: the {\it PowerFlux}
(see \cite{S6PowerFlux} and references therein), the {\it FrequencyHough}
\cite{VSRFH}, the {\it Skyhough} \cite{S5Hough} and the {\it Time-Domain
$\mathcal{F}$-stat} \cite{VSR1TDFstat}. The pipelines employ a variety of
algorithmic and parameter choices e.g., they primarily use either the frequency
or time domain data, adopt different coherence times used in first-stage data
processing (from 1800 s to 6 days), and treat differently the narrow spectral
artifacts (''lines'').
\begin{figure}[h]
\begin{minipage}{\linewidth}
\centerline{\includegraphics[clip,trim=0 {0.02\textheight} 0 {0.07\textheight},width=0.8\linewidth]{figures/O1_full_ul_wide.pdf}}
\end{minipage}
\caption{O1 all-sky upper limits for continuous gravitational waves from the {\em PowerFlux} pipeline. The upper (yellow) curve shows worst-case (linearly polarized) $95$\%~CL upper limits. The lower (grey) curve shows upper limits assuming a circularly polarized source.}
\label{fig:o1allsky}
\end{figure}
Outliers that survive all stages of any of the four pipelines are examined
manually for contamination from known, or possibly new, instrumental artifacts.
Survivors of this procedure are subjected to additional systematic
follow-up used for Einstein@Home searches \cite{ehfu}. Upper
limit results are presented in Fig.~\ref{fig:o1allsky}. The lowest upper
limits on worst-case (linearly polarized) strain amplitude $h_0$ are  $\simeq
4\times 10^{-25}$ near 170\,Hz. For a circular polarization (most favorable
orientation of the source), the smallest upper limits obtained are $\simeq
1.5\times 10^{-25}$.

In addition, several studies from the Initial Detector Era (LIGO S6 and Virgo VSR2, VSR4
runs) were recently published. They include an all-sky Mock Data Challenge
based on the LIGO S6 data \cite{AllSkyMDC}, a directed search towards nine
supernova remnants \cite{S6SNRPaper}, the Orion spur \cite{orionspur}, the
globular cluster NGC 6544 \cite{S6GlobularCluster}, as well as the deepest
all-sky survey for continuous waves from the Initial Detector Era, the S6
Einstein@Home search in the $[50, 505]$ Hz range \cite{EAHS6}. The reason we
see merit in publishing the `old' results is to gather experience, test
algorithmic improvements and develop new methods using the well-understood
data. These new tools are now being used in the O1 (and soon, the O2)
searches.

\section{Plans for the future} \label{sect:plans}

The algorithmic and implementation-related improvements acquired during the
Dark Ages (2011--2015) will be used to expand the `standard' targeted searches
for high-value targets (Sco X-1, Cas A, Vela Jr and G347 supernov{\ae}
remnants, Crab and Vela pulsars) and to speed up the massive all-sky searches
with relatively simple source models (aligned triaxial ellipsoid,
Eq.~\ref{eq:triaxial}). Additionally, we plan to search for signals with more
complicated, realistic morphology. The models include inclined rotating neutron
stars, which emit gravitational waves at multiple frequencies at once (e.g., at
$f$ and $2f$), transient continuous gravitational waves emitters (phenomena
that may last for weeks to months, and are caused by neutron-star instabilities
e.g., the r-modes), and search for non-tensorial gravitational waves. In order
to capture the richness of physical processes will are also improving the
loosely-coherent methods taking into account the neutron-star frequency
wandering, glitches, and a possible mismatch between the gravitational-wave spin
frequency parameters and the parameters inferred from the electromagnetic
observations.

\section*{Acknowledgments}
This work was partially supported by the Polish NCN grant no. UMO-2014/14/M/ST9/00707
and ASPERA/NCN grant 2013/01/ASPERA/ST9/00001.

\section*{References}

{\small

redpajama_set_name: RedPajamaArXiv


text:
Silicon based near infrared tunable filters based on liquid crystals
Complementary metal-oxide-semiconductor-compatible tunable Fabry-Perot microcavities filled with liquid crystals (LCs) were realized and studied in the near-infrared region. The microcavities were produced by chip bonding technique, which allows one to infill LC between two [SiO(2)/Si](n) lambda/4 (lambda = 1.5 mum) Dielectric Bragg Reflectors separated by 950 run thick SiO(2) posts. The Dielectric Bragg reflectors were realized on Si or SiO(2) substrates Liquid crystals with positive and negative dielectric anisotropy were used, i.e. MerckE7 (Deltaepsilon = 13.8) and Merck-6608 LC (Deltaepsilon = -4.2). Mirror-integrated electrodes allow an external bias to induce an electrical field and to tune the LC properties and, hence, the microcavity resonance. Electric-field-induced shifts of the second-order cavity modes of similar to120 nm and similar to50 nm were obtained for Merck-E7 and Merck-6608 LC, with driving potentials of 5 V and 10 V, respectively. The transmittance at the cavity resonance is typically in the order of 10%. Simulation of cavities allows to identify surface roughness of the Dielectric-Bragg-Reflectors as the major origin of the transmission losses. The switching behavior of microcavities filled with E7 were studied as function of applied fields. Both switch-on t(on) and switch-off t(off) times were measured and were found to be lower than 5 ms.
Titolo: Silicon based near infrared tunable filters based on liquid crystals
A. Mezzetti
G. Pucker
M. Crivellari
C. Kompocholis
P. Bellutti
A. Lui
Daldosso, Nicola
F. Riboli
M. Saiani
Z. Gaburro
L. Pavesi
PROCEEDINGS OF SPIE, THE INTERNATIONAL SOCIETY FOR OPTICAL ENGINEERING
Abstract: Complementary metal-oxide-semiconductor-compatible tunable Fabry-Perot microcavities filled with liquid crystals (LCs) were realized and studied in the near-infrared region. The microcavities were produced by chip bonding technique, which allows one to infill LC between two [SiO(2)/Si](n) lambda/4 (lambda = 1.5 mum) Dielectric Bragg Reflectors separated by 950 run thick SiO(2) posts. The Dielectric Bragg reflectors were realized on Si or SiO(2) substrates Liquid crystals with positive and negative dielectric anisotropy were used, i.e. MerckE7 (Deltaepsilon = 13.8) and Merck-6608 LC (Deltaepsilon = -4.2). Mirror-integrated electrodes allow an external bias to induce an electrical field and to tune the LC properties and, hence, the microcavity resonance. Electric-field-induced shifts of the second-order cavity modes of similar to120 nm and similar to50 nm were obtained for Merck-E7 and Merck-6608 LC, with driving potentials of 5 V and 10 V, respectively. The transmittance at the cavity resonance is typically in the order of 10%. Simulation of cavities allows to identify surface roughness of the Dielectric-Bragg-Reflectors as the major origin of the transmission losses. The switching behavior of microcavities filled with E7 were studied as function of applied fields. Both switch-on t(on) and switch-off t(off) times were measured and were found to be lower than 5 ms.

redpajama_set_name: RedPajamaCommonCrawl


text:
Beloved Incarcerated
Prisoner Art
Prisoner Poetry
Letters/Testimonies
The Christian Difference
Thoughts from Chaplain Lyons regarding a prison ministry conference he attended in November 2000
Chaplain Emmett Solomon, Director of "Restorative Justice Ministries Network" has had 30 years experience working under the Texas Department of Corrections. Chaplain Solomon shared many poignant facts about why our correctional system does not work, and also some positive corrections that Restorative Justice and others are doing that are proving to make a difference in the correctional setting.
Chaplain Solomon confirmed what most of you know, that is, that most inmates only get worse while they are in prison. His basic message was that most people who are habitual criminals (institutionalized the majority of their lives) have never had a family support system to teach them what they need to know to become responsible adults. And, that most criminals have the maturity of an adolescent.
He stated that it takes a parent to impart four virtues into their children to raise them correctly: Love, guidance, nurturing, and discipline. Most criminals have only received a vain attempt of guidance from their parents and an imbalance of discipline. With-out love and nurturing, they can never grow and mature into responsible men and women.
Chaplain Solomon asked us the question, "And what do these people receive in prison?" The obvious answer was, "Only guidance and discipline".
He mentioned that there is no real way out of the cycle that entraps these individuals in their immaturity. They do not learn how to make responsible decisions while incarcerated. They are told what to do and when to do it. If
they do not do what they are told, they are disciplined severely. Without experiencing some love and nurturing, the cycle of destruction continues.
However, he did mention that the correctional system is beginning to acknowledge that love and nurturing can change the attitude and character of a criminal. He documented that the Texas Department of Corrections has
observed that when they treat men and women in prison who are considered incorrigible with some dignity, love and nurturing, many of these inmates become manageable, and can function in the main line with the other inmates.
Also, Chaplain Solomon stated that the Texas Department of Corrections is seeing that giving offenders the opportunity to accept Christ, being reconciled with the victim by asking for forgiveness, and making restitution, can generate true rehabilitation.
Even with the above being true, Chaplain Solomon emphasized that a correctional institution will never really be designed to offer anything more than discipline. He added that society does not want to minister to those incarcerated, but rather wants to see them punished severely for their crimes. Not that punishment is wrong, but the right type of punishment needs to be administered and restitution/reconciliation is an intricate part of proper correction.
Society's fear of approaching the incarcerated is so acute that society feels safer with the "out of sight, out of mind" approach. However, it's not that simple.
Almost everyone who is incarcerated will get out of prison or jail. If inmates' lives are not changed while incarcerated, they will victimize society again.
This is why the church is so important. The correctional system's focus will never really be on love and nurturing, but the church's focus should be. We as Christians have the answer, and we should make ourselves visible to the correctional system, to reinforce Christ's ministry of repentance, restitution, restoration and reconciliation.
Chaplain Art Lyons'
Re-Entry Website
CPP is a faith based ministry which depends on donations to help with the costs of mailing. We need your help to keep this service available to inmates without charge. If you believe this work is worthy, please consider giving!
Thank you in advance and may God bless you!
Send stamps or checks made out to:
Christian Pen Pals
Copyright © 2021. All Rights Reserved. Christian-PenPals.com
Designed by HeDoesWebDesign.com.


I have a problem with step 2, I'm highly allergic to citric acid and citrus foods (coconut oil included) what would you suggest as a substitute? Please reply via Email at slc7898@aol.com my name is Shelly. Thanks! I am loving your page by the way.
I think any oil you tend to use for pancakes would work. You could use butter or safflower oil. If you have another oil you prefer for skillet cooking, you could use that, too.
Dear Carissa, I clicked on the link as the title "gultenfree pancakes" was interesting to me, since I am gluten intolerant (at the full blown disease stage). I don't wnt to ruin your pleasure offering gluten free advice, however I feel I MUST inform gluten intolerant people (and you) that oats and oatmeal does contain gluten! Before I was diagnosed and due to the dily stomach aches (back then I did not even have the full blown disease yet) several people were encourageing me to make porridge as supper or late evenning treat (to ease pain and since oat is so healthy-if you can stand it). I was just getting sickr and sicker, and althought I did not know the reason, I simply found out, getting the porridge out of my diet (and the morning cecreals and muesli-type stuff with my yoghurt) helped. (However the disease continued with wheat and rye-based products I ate since I did not know why I had problems and the doctors were looking for fodd allergies, nobody thought of gluten intolerance).
Thanks for your note. Oats themselves do not contain gluten although many food manufacturers process their oats on the same machinery used to process wheat. Those sensitive to gluten can usually still eat oats but may need to purchase certified gluten free oats which will not have the cross contamination issue.


BALTIMORE (AP) All-Star reliever Darren O'Day and the Baltimore Orioles have completed a $31 million, four-year contract.
The Orioles announced Monday that the 33-year-old free agent had re-signed with the team. He will make $6 million next year, $7 million in 2017 and $9 million the following two seasons. There will be $1 million deferred each year, with the deferred money payable in four installments each July 1 from 2020-23.
O'Day was an All-Star last season when he went 6-2 with six saves and a 1.52 ERA in 68 games. The submarining right-hander struck out a career-high 82 in 65 1-3 innings.
O'Day is 31-13 with 14 saves and a 2.31 ERA in 459 games in an eight-year career with the Angels, Mets, the Rangers and Orioles. He joined Baltimore in 2012.
Infielder Rey Navarro was designated for assignment. He hit .276 in 10 games for Baltimore last season.


text:
Description. Lang: en
The River Mersey () is a river in the North West of England. Its name is derived from the Anglo-Saxon language and translates as "boundary river". The river may have been the border between the ancient kingdoms of Mercia and Northumbria and for centuries it formed part of the boundary between the historic counties of Lancashire and Cheshire.The start of the Mersey is at the confluence of the River Tame and River Goyt in Stockport. It flows westwards through the suburban areas of south Manchester, then into the Manchester Ship Canal at Irlam, becoming a part of the canal and maintaining the canal's water levels. After 4 miles (6.4 km) the river exits the canal, flowing towards Warrington where the river widens. It then narrows as it passes between the towns of Runcorn and Widnes. From Runcorn the river widens into a large estuary, which is 3 miles (4.8 km) across at its widest point near Ellesmere Port. The course of the river then turns north as the estuary narrows between Liverpool and Birkenhead on the Wirral Peninsula to the west, and empties into Liverpool Bay. In total the river flows 70.33 miles (113 km).
A railway tunnel between Birkenhead and Liverpool as part of the Mersey Railway opened in 1886. Two road tunnels pass under the estuary from Liverpool: the Queensway Tunnel opened in 1934 connecting the city to Birkenhead, and the Kingsway Tunnel, opened in 1971, to Wallasey. A road bridge, completed in 1961 and later named the Silver Jubilee Bridge, crosses between Runcorn and Widnes, adjacent to the Runcorn Railway Bridge which opened in 1868. A second road bridge, the Mersey Gateway, opened in October 2017, carrying a six-lane road connecting Runcorn's Central Expressway with Speke Road and Queensway in Widnes. The Mersey Ferry operates between Pier Head in Liverpool and Woodside in Birkenhead and Seacombe, and has become a tourist attraction offering cruises that provide an overview of the river and surrounding areas.
Water quality in the Mersey was severely affected by industrialisation, and in 1985, the Mersey Basin Campaign was established to improve water quality and encourage waterside regeneration. In 2009 it was announced that the river is "cleaner than at any time since the industrial revolution" and is "now considered one of the cleanest in the UK". The Mersey Valley Countryside Warden Service manages local nature reserves such as Chorlton Ees and Sale Water Park. The river gave its name to Merseybeat, developed by bands from Liverpool, notably the Beatles. In 1965 it was the subject of the top-ten hit single "Ferry Cross the Mersey" by Gerry and the Pacemakers.
River Mersey Map
River Mersey Facts
River Mersey Cruise
River Mersey Stockport
River Mersey Pollution
River Mersey Manchester
River Mersey Liverpool
River Mersey Fishing
River Mersey Song
River Mersey River in England
Mersey River River in Nova Scotia, Canada
Mersey River River in Australia
www.engineering-timelines.com
www.isle-of-man.com
www.merseyreporter.com
www.visitmyharbour.com
pubmed.ncbi.nlm.nih.gov
www.ncbi.nlm.nih.gov
River in England
Desc: The River Mersey is a river in the North West of England. Its name is derived from the Anglo-Saxon language and translates as "boundary river".
Wiki: https://en.wikipedia.org/wiki/River_Mersey
Type: Thing, Place, RiverBodyOfWater, TouristAttraction, BodyOfWater
Mersey River
River in Nova Scotia, Canada
Desc: The Mersey River, formerly known as Rivière Rossignol by the Acadians, is a river in Nova Scotia, Canada. It is named after the River Mersey in Liverpool, England.
Wiki: https://en.wikipedia.org/wiki/Mersey_River_(Nova_Scotia)
Type: Thing, Place, RiverBodyOfWater, BodyOfWater
River in Australia
Desc: The Mersey River is a river on the north-west coast of Tasmania, Australia. The city of Devonport is situated at the river's mouth on Bass Strait.
The source of this river is Lake Meston.
From here the river feeds itself into Lake Youd.
Wiki: https://en.wikipedia.org/wiki/Mersey_River_(Tasmania)


text:
class Prometheus < Formula
  desc "Service monitoring system and time series database"
  homepage "https://prometheus.io/"
  url "https://github.com/prometheus/prometheus/archive/v1.0.1.tar.gz"
  sha256 "b1a74b77d71521ac5439eccc1eec97b0106c350d9bf6f02d694bd40142ab0620"

  bottle do
    cellar :any_skip_relocation
    sha256 "0847327c35dfddcd0c4a2d6c3e14fb81ed3e6b688c61a011915c6ef20b377770" => :el_capitan
    sha256 "9b922b98bf15522e0d26a0f5c43f7275a2eed7c60399db8d2398e8c268c2c044" => :yosemite
    sha256 "affeb9eb6485eece9fa4fbf079346458eee83c6dfa92381d2d9d6c78e94d96c5" => :mavericks
  end

  depends_on "go" => :build

  def install
    ENV["GOPATH"] = buildpath
    mkdir_p buildpath/"src/github.com/prometheus"
    ln_sf buildpath, buildpath/"src/github.com/prometheus/prometheus"

    system "make", "build"
    bin.install %w[promtool prometheus]
    libexec.install %w[consoles console_libraries]
  end

  test do
    (testpath/"rules.example").write <<-EOS.undent
    # Saving the per-job HTTP in-progress request count as a new set of time series:
      job:http_inprogress_requests:sum = sum(http_inprogress_requests) by (job)
    EOS
    system "#{bin}/promtool", "check-rules", testpath/"rules.example"
  end
end

redpajama_set_name: RedPajamaGithub


Detroit Red Wings center Joakim Andersson is out indefinitely with a broken foot sustained when he was hit by Dominic Moore's shot during the second period of Detroit's 3-0 loss to the New York Rangers on Sunday.
The Red Wings have five centers on injured reserve: Andersson, Pavel Datsyuk (sore right knee), Henrik Zetterberg (back surgery), Darren Helm (upper body) and Stephen Weiss (sports hernia surgery). Detroit acquired veteran David Legwand from the Nashville Predators at the NHL Trade Deadline and will call up Cory Emmerton from the Grand Rapids Griffins of the American Hockey League.
Riley Sheahan and Luke Glendening are the other healthy centers on a team fighting to make the playoffs for a 23rd consecutive season.
"It's a bad position, I guess," Andersson told reporters.
Andersson has seven goals and 15 points in 58 games for the Red Wings this season.


text:
Composing the score for Robin Robin (Aardman / Netflix)
Robin Robin is out now on Netflix and you can listen to the
original motion picture soundtrack album now on Spotify.
The Animated Journey In 2006 my brother Mikey Please began making short animations, first for fun and then at college (where he also had fun). Short beautiful animated experiments with stories he'd written. He turned to me for his source of creatively matched (free) musical and sound design labour. From the shadow puppet quirkiness of Glen's Gloves, to the comically twisted Crone. In 2009 Mikey went to the RCA to do a masters in Animation and his final project was The Eagleman Stag, based on a short story he'd written years earlier. I had fun collecting all the sounds from our childhood home and garden, and also meeting and collaborating with Beth Porter for the first time who was part of a string quartet called The String Beans (now Red Carousel) who I used to record some of the score for the film using a cheap microphone cellotaped to the side of a stool. The film went on to win a BAFTA the following year and (was even long listed for an Oscar) and spurred Mikey on a series of other ambitious animated shorts, Marilyn Myller and then into colour for Alan The Infinite, now collaborating with his friend and co-director, Dan Ojari. The scores became progressively more ambitious too, involving two microphones strapped to a chair and a carousel of musicians, flutists to opera singers, booked for 10 minute slots at a time to come and stand in front of this chair and play their musical contributions into the evolving scratch orchestra.
The Pitch and Scratch In 2019 Mikey told us that Dan and him had been pitching to Aardman a seasonal musical called Robin Robin, about a baby Robin that gets adopted by a family of mice. Aardman had bitten and shortly after Beth and I were asked to spend a couple of weeks writing scratch music to help them develop the story. We were on tour with our daughter Molly, and so we spent the best part of two weeks in other people's kitchens writing and recording ideas for the main songs in the film. We only had one mic (a nice little Gefell M300 for those who want to know), but this time we had a mini mic stand! There were washing machines, Molly's watching of films, cars, alarms in the background, but I think what is amazing is that most of those recordings actually made it into the final film. They were only ever intended as scratch recordings, but I think the pressure of trying to convince the directors and Aardman that they should like what we did meant that we actually tried to make them sound nice and "orchestral". There was also a spontaneity about them which would have been difficult for us to re-capture. A year or so down the line to the orchestral overdub recording session at Realworld, with the Bristol Ensemble under the baton of Drew Morgan, those free-flow recordings that made the final cut presented huge challenges to Drew as he conducted his heart out to keep the players in sync with our whimsical timings. What you get at the end though is something that still (we think) retains a freshness, despite it passing through an industrial-scale musical machine, because you really are hearing the first moments those notes were played in those recordings, but they are now backed by brass sections and supported by Welsh men's choirs. Beth used to clean the toilets at Realworld as her first job out of uni, so it was quite a moment for her to be sitting in the control room there in the composer's chair.
The Writing and Recording
After those first few weeks of scratch music writing we ended up being offered the job of scoring the whole film. It could not have come at a more fortuitous time as our year's plans for touring in the US had just been scuppered, along with everyone else plans, due to the encroaching pandemic. Spreadsheets were made, cues listed out, stories and animatics began appearing and we set to work cue by cue. Beth and I write together most of the time so our main issue was childcare, but we managed to get about an hour and a half a day as Molly donned her headphones and we made use of our Disney+ Channel subscription. I assume we work in a very non-standard way for film composers. Nothing is done on the computer, nothing in midi. Everything is recorded, ideas go down as if we are in the studio, and what comes out of the day is an actual recording which we know full well will not make it into the final film, as even if they like it the chances are very high that all the timings will change and we'll have to re-do it. It's a crazy way to work I'm sure, but it's how we it.
The songs were an interesting challenge as they came with pre-written lyrics by the directors, with their own intrinsic tempos and rhythmic structures that we had to unpick and weave into a melody. In many ways it was quite liberating to have that part of the process done. Many musical iterations were written but we often all ended up going back to the first one. When it came to recording we managed to get one session in person with the actors Gillian Anderson, Richard E Grant and Bronte Carmichael before everything went into lockdown and the rest of the sessions had to be conducted over Zoom. Unfortunately we never got to meet Adeel Akhtar.
Once all the cues had been written, and re-written, and re-timined to the new animatic, and re-recorded again to fit the new timings, and then re-timed and re-written and then re-timed and then re-written and recorded (all using the same mic) I headed down to Realworld to record a handful of soloists to augment our recordings with instruments we wanted but couldn't play ourselves. Long time collaborator Jools Scott played piano as his baby slept upstairs, Beth's sister Hannah Porter came to play violin and flute, great friend and player Pete Judge came in with his selection of brass instruments for Magpie, and Chris Cundy brought his bass clarinet to play the cat. We also recorded expert double bassist (the Whoo-mans) Emma Smith up in Dumfries on the way home. A Peter And The Wolf affair. My one epic lockdown trip was to purchase a dulcitone (an old mellow tune-fork piano) from The Unthanks to be Robin's instruments after a discussion with the directors. When I sent them a sample recording they immediately didn't like it, and so Beth's recorder became Robin's instrument. Luckily I quite like the dulcitone and so it stays in the studio.
Finally we handed everything over to Jools Scott and Adam Langston - two wonderful composers in their own right, to arrange extra parts for the orchestra to overdub at various points in the score. Huge string swells, percussive smashes, collier brass pads and angelic choirs. Each had to be recorded in it's own section due to corona restrictions on space which we did at Beth's old haunt Realworld, and at a new studio called Challow Park near Wantage for the slightly larger string section. The children's choir we had to record remotely which was beset with technical problems, but we somehow managed to get everything done. As each new layer came in the sound grew and grew, textural layers began to stack on to our quirky recordings but always leaving holes for all the others underneath to be heard. It was like travelling through a cloudscape - one thing envelopes you and then dissipates to show the view all around. The closest we'll get to magic.
The whole team at Aardman were brilliant - and what a treat to be carried through it by them.
The film Robin Robin is out now on Netflix, and if you would like to listen to the full score in all it's epic nakedness then that is available now on Spotify (and we hope on vinyl in the not too distant future on Lakeshore Records).
If you would like to find out more about our film score work, please visit: https://www.porterandplease.com


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DEALING WITH YOUR SPOUSE'S AFFAIR - Brian D. Perskin & Associates P.C.
Most people go into a marriage believing that they would never be the victim of an affair. While for some people, infidelity is not a deal breaker, for others, it can be the cause of an immediate divorce. For certain individuals, they don't care about reasons or excuses. For them, cheating means divorce.
However, if you are an individual that considers other factors, such as finances and children, when considering divorce after infidelity, you're not alone. There are many things to think about after a spouse cheats and you should not feel pressured by friends or family to immediately divorce them.
The first thing you should do following a spouse cheating is consider the past and current quality of the marriage. If you feel as though your marriage has been on the rocks for years, cheating may have been the final tipping point in your relationship and may be reason for divorce. However, if your marriage was in a good state prior to the affair, you may have other things to consider prior to divorce.
There are two types of recovery following an affair which include personal recovery and marriage recovery. Personal recovery is exactly what it sounds like- it means taking time for yourself and healing from the pain of a spouse cheating. Personal recovery is more than just "getting over it", it includes allowing yourself to have hurt feelings and working through them.
On the other hand, marriage recovery is not exactly what it sounds like. This type of recovery means changing your marriage after infidelity and working through the problems that caused the spouse to change in the first place. If all you do after the affair is move on and go back to normal in the relationship, your marriage will continue to be toxic. You also need to decide if the marriage is worth working through and putting in effort to save. If not, considering a divorce is a viable option.
CAN YOU FULLY RECOVER AFTER AN AFFAIR?
While this is a question that can only be answered on an individual basis, many people find that they can never fully trust their spouse again following an affair. If you feel as though you will have trust issues for the rest of the relationship, contacting an experienced divorce attorney can help. Lawyers that specialize in divorce and family law can weigh your options and help you work through it.
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