text:
Louis Clappier (* um 1921; † 1956 in Paris) war ein französischer Publizist und Schriftsteller.

Leben
Clappier war Herausgeber der Zeitschrift Allemagne d'aujourd'hui und ist unter anderem als Übersetzer von Wolfgang Koeppen und als Teilnehmer der Gruppe 47 bekannt.

Werke
 Festung Königsberg. Übersetzt von Werner von Grünau. Kiepenheuer & Witsch, Köln / Berlin 1952 (Originaltitel: Place-forte Koenigsberg)

Übersetzungen
 Wolfgang Koeppen: Pigeons sur l'herbe. (Übers. von Tauben im Gras.) Paris: Laffont, 1953.

Weblinks
 Literary Landmarks of 1956. A Necrology.

Publizist
Autor
Franzose
Geboren im 20. Jahrhundert
Gestorben 1956
Mann

redpajama_set_name: RedPajamaWikipedia


1997 Infiniti J30 Service Repair Manual Software - Fulfillment by Amazon (FBA) is a service we offer sellers that lets them store their products in Amazon's fulfillment centers, and we directly pack, ship, and provide customer service for these products.. ATSG GM THM 4L60-E Transmission Update Technical Manual is necessary to diagnose, overhaul and/or repair the 4L60E transmission. GM THM 4L60-E Transmission Update Handbook covers engineering changes that have occurred from 1993 to 2003, parts affected by the change, interchangeability and part numbers.. Motor Trend reviews the 2003 Dodge Viper where consumers can find detailed information on specs, fuel economy, transmission and safety. Find local 2003 Dodge Viper prices online..
Motor Trend reviews the 2004 Jeep Grand Cherokee where consumers can find detailed information on specs, fuel economy, transmission and safety. Find local 2004 Jeep Grand Cherokee prices online..


text:
Salame steht für:
 Salami, eine Wurst
 Beni-Salame, auch Benisalame, Dorf in Ägypten und Ausgrabungsstätte (Merimde-Kultur)

Salame ist der Nachname von:
 Georges Salame, libanesischer Skifahrer
 Ghassan Salamé (* 1951), libanesischer Politiker
 Hadi Salame (* 1981), libanesischer Fußballschiedsrichter
 Jean Salame, französischer Kanute
 Jihad Salame, libanesischer Leichtathlet
 João Salame Neto (* 1962), brasilianischer Politiker
 Khodor Salame, libanesischer Fußballspieler
 Léa Salamé (* 1979), französisch-libanesische Journalistin
 Maty Salame, senegalesische Leichtathletin

siehe auch:
 Salam
 Salamé
 Salameh


First podcast January 12, 2009.
Our talk talk acclaimed short story writer James Powell!
HERE are the vintage shownotes.
I've been listening to these for hours today. The audio dramatizations are actually pretty good. The short stories tend to be very solid too (and are mostly read by their authors). Sound quality varies though and sometimes the recording level volume is set far too low. Additionally, the proof-listening is occasionally very shoddy (with repeated lines remaining unedited). The latest episode (#7) has three stories all based on the same newspaper article. The results are mixed, but I really like the idea of stories based around a story seed like that. In fact, it reminds me of something John Joseph Adams and David Barr Kirtley were talking about in a recent Geek's Guide to the Galaxy podcast. They mentioned the John W. Cambpell story seed that lead to the writing of Isaac Asimov's Nightfall and Robert A. Heinlein's Orphans Of The Sky. Two SF stories that are both very different and very terrific.
My favourite Ellery Queen Mystery Magazine podcast episode so far is #5, Dear Doctor Watson, a Steve Hockensmith short story. Its a kind of Sherlockian pastiche set in the Victorian West. It's protagonist a kind of amateur Sherlock Watson team that's only half-hampered by being illiterate and in Montana. Dear Doctor Watson is both fun and well read by two narrators.
I truly hope to see the "Ganelon" stories by James Powell and the "Black Widowers" tales by Isaac Asimov showing up in future episodes. They're the absolute tops!
Episode 1: Cut! Cut! Cut!
Ellery Queen receives a phone call from a murder victim in this clever play involving a witness of another species. First published in Ellery Queen's Mystery Magazine September 1956 issue.
A nosy neighbor alerts police to suspicious digging in the garden next-door—and she isn't the only one to get an unexpected comeuppance. First published in EQMM in November 2001.
A TV writer goes missing, leaving her show's star without a script and opening up a perfect scenario for murder. In this fourth installment in her series of Diana Poole mysteries, former Hollywood actress Melodie Johnson Howe takes a penetrating look at the off-stage life of a TV idol. First published in EQMM June 2003.
Ellery Queen returns in a case involving a cryptic dying message. First published in EQMM in February, 1953. The story later appeared under the titles Murder In The Park and The Mystery Of The 3 Dawn Riders.
A pair of Old West cowboys try to prove they're worthy of joining a detective agency by retrieving an incriminating letter. But things are not all they appear to be in Missoula, Montana, circa 1890… First published in the February 2007 issue of EQMM.
The solving of so-called "impossible crimes" is the hallmark of Edward D. Hoch's series character Dr. Sam Hawthorne. In this episode, the New England country doctor is on board a night train when a body is discovered in its locked caboose. First published in EQMM in May, 1976.
Three stories (Say That Again by Peter Lovesey, The Old Story by Liza Cody, and Wheeze by Michael Z. Lewin) that take their lead from a single newspaper article provide an entertaining look at how a common creative impetus can take the imaginations of different writers in wonderfully different directions. Includes a short interview with the authors, all leading writers of suspense, recorded at the 2009 Bouchercon World Mystery Convention.


DROITWICH judo club Kazoku-Kan enjoyed success in the Midland Area Mix and Match competition at Birmingham's Erdington Academy.
Luke Phillips put on an outstanding display by winning all of his contests with conviction to secure the gold medal.
His younger brother Jordan, in his first competition for the club, put up a fine effort and walked away with gold as well.
Harry and Sian Evans, the last in the junior category, had tough competition but both returned with bronze medals.
In the senior category club head instructor Robert Alloway won both his contests with a stunning shoulder technique and then a hold-down to win the gold.


Bill Peet, artist-writer and longtime member of the Walt Disney production company, has chosen a highly appropriate fable, the 1938 T.H. White book of the same title, for screen adaptation for the youngsters. It emerges as a tasty confection.
The feature-length cartoon demonstrates anew the magic of the Disney animators and imagination in character creation. But one might wish for a script which stayed more with the basic story line rather than taking so many twists and turns which have little bearing on the tale about King Arthur as a lad.
Key figures are the boy who is to become king of England because he alone has the strength to remove the sword embedded in a stone in a London churchyard (he goes by the name of Wart), and Merlin, a magician and prophet, who's alternately wise and somewhat nutty. Others include the villainess Mad Madam Mim, who turns out to be a nice old dame, an English nobleman, a kind-hearted owl, flora & fauna, etc.
The songs by Richard M. and Robert B. Sherman are in the familiar Disney cartoon groove with such titles as 'Higitus-Figitus,' 'Mad Madam Mim' and 'The Legend of the Sword in the Stone.' They're agreeable tunes and go along nicely with the animated action.
Crew: (Color) Available on VHS, DVD. Extract of a review from 1963. Running time: 75 MIN.


Based in south London, TheNeverPress is an independent publishing house specialising in fiction, though we're not averse to venturing into other fields when the right project comes along.
We've got a stimulating slate of books in production – not just novels, but also comics, short story collections, graphic novels, children's picture books and poetry. We value our independence and plan to release a few publications each year in a unique, modern fashion: online serialisations, blogs about things we like – and that you might too – reports from local events, maybe a podcast or two. We might not be a publishing behemoth right now, but that's the point. We're just going our own way.
Our books are now available worldwide through Amazon and we're building a nice in-house store so you can purchase directly from this site, and we're hoping to be stocked by local bookshops. Who knows – we might even pop up at a stall near you.
We're artists, writers, coders, designers and bloggers who want to create a label that nurtures each project's vision. Our aim is to lay a strong foundation of trust and encouragement: whatever the idea, we'll give it a fair crack of the whip.
Feel free to drop us a line if you want to chat about any of our projects… or, indeed, your own.
As a wee lad, Graham wanted to be a pilot, a butler, a filmmaker and an author. The only one that stuck with him was author. He likes to ponder and plan, and though they say a plan is just a list of things that never happen he does have a firm roadmap for where he, and TheNeverPress, are going. He has a slate of another 10 books queued up for the next five years, each one planned and developed and just waiting for the start date to roll around. After that, he has a nebulous plan for future books – 30 or 40 more brewing away. Alongside writing, he loves cooking roasts and The Cure. Graham also takes comfort in the fact that although he is the wrong side of 35, he is always the right side of the bar.
Hayley Joan is a UI artist in the regular hours, outside of those she is a designer, a painter, a photographer, a DJ, a guitarist, an angel at the mic and a demon at the synth. Basically she can do anything...although we haven't tested her at canasta, yet.


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text:
\section{Introduction}
Coalescing systems of stellar mass binary black holes (BBHs) are
among the most likely candidates for the first detection of
gravitational waves (GWs) \citep{bbh1,buo03}. Their enormous
predicted luminosities $\sim 10^{23}L_{\odot}$, would allow future
ground-based interferometric GW detectors, such as Advanced LIGO
\citep{aligo} and Advanced Virgo \citep{avirgo} or third generation
instruments such as the Einstein Telescope \citep[ET;][]{et}, to
probe these sources out to Gpc distances. In this paper, we are
motivated by recent increased rate estimates \citep{metal} to
explore the possibility that a population of BBHs could form a
detectable stochastic GW background (SGWB) signal for these
instruments.

SGWBs can result from the superposition of populations of unresolved
primordial \citep{Grishchuk:1974ny} or astrophysical sources
\citep[see][for a recent review]{regimbau11}. Astrophysical SGWB
signals are important for at least two reasons. Firstly, they
contain rich information on the global properties of source
populations, such as their source rate evolution, their mass ranges
and their average energy emissions. Secondly, a dominant continuous
astrophysical background could mask the relic SGWB signal from the
very early Universe \citep[see][for reviews]{Maggiore,Buonanno}.

Mergers of binary neutron stars have been suggested as sources of
potentially detectable SGWBs \citep{Regimbau06,Regimbau07}. Recent
observations of BH-Wolf-Rayet (WR) star systems \citep{Crowther} and
new estimates in the metallicity abundances of star forming galaxies
\citep{2008MNRAS.391.1117P} imply that the Galactic merger rate of
BBHs may be of a similar order to that of binary neutron stars
\citep{metal}. Therefore, a population of more luminous BBHs could
produce a dominant background signal. Our aim is to explore upper
limits for a SGWB from coalescing BBHs over a range of rates and
system masses. We investigate the constraints future ground based
interferometric GW detectors will be able to place on the average
properties of the BBH population.

The paper is organized as follows. In Section 2 we discuss rate
estimates of coalescing BBHs and then derive cosmic source rate
evolution models for different star formation histories and minimal
delay times. In Section 3, source energy spectra for coalescing BBHs
are obtained using the template gravitational waveforms of
\citet{IMR} and \citet{spin_IMR}. We then calculate the BBH
background in Section 4 and discuss the detection regimes,
detectability and constraints on the parameter space of the
predicted background in Section 5. Finally, in Section 6 we present
our conclusions.

\section{Rates of BBH coalescences}
The discovery of BH-WR star systems within close proximity has
increased rate estimates of coalescing BBHs. There are presently two
known systems: NGC300 X-1, which lies at a distance of 1.8 Mpc and
is composed of a $\sim 20 M_{\odot}$ BH and a WR star of $\sim 26
M_{\odot}$ \citep{Crowther}; IC10 X-1 contains a BH of a mass at
least $23 M_{\odot}$ and a $\sim 35 M_{\odot}$ WR star, and lies
within 700 kpc \citep{Prestwich}. As WR stars are the progenitors of
Type Ib/c supernovae, if such systems survive the supernova
explosion, BBH systems will form and eventually coalesce within a
timescale of Gyrs \citep{Bulik08}.

Recent results from Sloan Digital Sky Survey, have indicated that
half of recent star formation involved galaxies with low metallicity
\citep{2008MNRAS.391.1117P}. This has a profound effect on the
coalescence rates of compact binaries containing BHs when one
considers that NGC300 X-1 and IC10 X-1 were both formed in low
metallicity environments.

Survival of BBH systems is highly dependent on whether they can
overcome two key obstacles in their evolution. Firstly, post natal
supernova kicks can disrupt a significant proportion of systems.
Secondly, orbital shrinkage during the common envelope phase when
the larger star transfers mass to its smaller companion, can cause
the stars to merge before they become compact objects. \citet{metal}
have shown through population-synthesis modeling that a lower
metallicity environment can suppress these two effects. Firstly,
observational evidence suggests that larger BH masses, which are
produced at low metallicity, are born with lower kick velocities
\citep{Mirabel,bhmass}. Secondly, in lower metallicity environments,
slower radial expansion occurs during the common envelope phase,
thus increasing binary retention. The greater fraction of systems
that can survive, in combination with a greater detection range from
more massive and hence luminous systems, has increased the detection
prospects of BBHs for ground-based interferometric GW detectors
\citep{metal}.

Previous estimates of the coalescence rate of BBHs formed through
isolated binary evolution in the field have ranged over orders of
magnitude, from $10^{-4}$ to 0.3 Mpc$^{-3}\rm{Myr}^{-1}$ with a
realistic value of $5 \times 10^{-3}\, \rm{Mpc}^{-3}\rm{Myr}^{-1}$
\citep{DCO,lsc_rate}. The effect of metallicity discussed above
increases the realistic estimate to $3.1 \times
10^{-2}\,\rm{Mpc}^{-3}\rm{Myr}^{-1}$ assuming a 50-50 mixture of
solar and $10\%$ solar metallicity and the most stringent
evolutionary scenario with respect to system survival \citep{metal}.
Unless we state otherwise, this rate (denoted as $r_{1}$) is adopted in our
calculations.

A higher estimate of $0.43\,\rm{Mpc}^{-3}\rm{Myr}^{-1}$ (denoted as
$r_{2}$) was obtained by assuming that all systems survive early
merger during the common envelope stage. We note that $r_{2}$ leads
to a detection rate for initial LIGO/Virgo of around 5 events per
year. A recent population synthesis study by \citet{Bulik08},
however, has demonstrated the formation of BBHs with high chirp
masses ($\sim 15 M_{\odot}$) from the two BH-WR systems, and has
yielded a similarly high rate of $0.36 \hspace{0.5mm}\rm{Mpc}^{-3}
\hspace{0.5mm} \rm{Myr}^{-1}$ corresponding to 3.6 detections a
year. They suggest that either currently employed searches are
insensitive to higher mass BBH inspirals or that there is an
additional aspect to the evolution of such systems that has not so
far been considered. To take account of this uncertainty, we take
$r_{2}$ as a higher rate.

\subsection{The cosmic rate evolution model}
The cosmic coalescence rate can be extrapolated from the local rate
density $r_0$ by assuming the rate tracks the star formation rate
(SFR). Explicitly, the differential GW event rate in the redshift
shell $z$ to $z + dz$ can be written as
\begin{equation}
dR = r_{0}e(z)\frac{dV}{dz}dz \label{dR},
\end{equation}

\noindent with $dV$ the cosmology dependent co-moving volume element given by

\begin{equation}
\frac{dV}{dz}=4\pi c\frac{r(z)^{2}}{H(z)},
\end{equation}

\noindent where the Hubble parameter $H(z)=
H_{0}[\Omega_{\Lambda}+\Omega_{m}(1+z)^{3}]^{1/2}$ and $r(z)$ is the
comoving distance related to the luminosity distance by
$d_{L}=r(1+z)$. We use the parameters $H_{0}=100 h\cdot
\rm{km}\hspace{0.5mm} \rm{s}^{-1}\hspace{0.5mm} \rm{Mpc}^{-1}$ with
$h=0.7$, $\Omega_{m}=0.3$ and $\Omega_{\Lambda}=0.7$
\citep{cosmology}.

Source rate density evolution is accounted for by the dimensionless
evolution factor $e(z)$, normalized to unity in our local intergalactic neighbourhood.
Following \citet{Regimbau09}, we define $e(z)=
\dot{\rho}_{\ast,c}(z) / \dot{\rho}_{\ast,c}(0)$ normalized to unity
at $z=0$ where
\begin{equation}
\dot{\rho}_{\ast,c}(z)= \int
\frac{\dot{\rho}_{\ast}(z_{f})}{(1+z_{f})} P(t_{d}) dt_{d},
\end{equation}

\noindent relates the SFR to the BBH coalescence rate. Here,
$\dot{\rho}_{\ast}$ is the SFR density in $M_{\odot}
\hspace{0.5mm}\rm{yr}^{-1} \hspace{0.5mm}\rm{Mpc}^{-3}$, based on
the parametric form of \citet{SFR}, derived from recent measurements
of the galaxy luminosity function. To allow for uncertainties in the
SFR, we also consider a recent model described in \citet{Wilkins},
obtained through measurements of the stellar mass density -- this
model gives a much lower rate for $z
> 1$. The factors $z$ and $z_f$ represent the redshift values of
BBHs merger and BBH system formation
respectively. The delay time for BBHs, $t_d$, is
given by the difference in lookback times between $z_f$ and $z$

\begin{equation}
t_{d}= \int_{z}^{z_f} \frac{dz'}{(1+z')H(z')}.
\end{equation}

\noindent Here $P(t_{d})$ is the probability distribution of delay
times. For this we take the form, $1/t_{d}$, with a lower cutoff
$t_0$ at 100 Myr as suggested by current population synthesis
studies \citep{ps02,ps06,Dominik}. To account for uncertainty in the
lower cutoff and possible correlation between $P(t_{d})$ and BBH
chirp masses, we additionally consider a longer minimal delay time
of  $t_0 = 500$ Myr (T. Bulik, private communication).

Figure 1. shows the cosmic rate evolution factor $e(z)$ of BBH
coalescences for different SFRs and minimal delay times. Although
the models show some variation in peak $z$, we show in section 4
that the magnitude of the background is largely dependent on $r_0$
rather than the form of $e(z)$.

\section{The GW energy spectrum of coalescing BBHs}
The evolution of a coalescing BBH is traditionally divided into
three phases: \emph{inspiral}, \emph{merger} and \emph{ringdown}.
While the early inspiral and ringdown phases can be approximated
analytically by post-Newtonian expansion and perturbation theory, to
model the late inspiral and merger requires a numerical solution of
the Einstein equations. In the last few years breakthroughs in
numerical relativity have enabled the inspiral-merger-ringdown
evolution of BBH coalescences to be modeled with high accuracy for a
broad space of parameters \citep[see, e.g.,][for
reviews]{han09,bbh_status}.

For the complete evolution history of coalescing BBHs,
phenomenological waveforms can be constructed by frequency domain
matching of post-Newtonian inspiral waveforms with coalescence
waveforms from numerical simulations
\citep{ajith07,buo07,pan08,san10}. Such waveforms share a common
feature, in that the Fourier amplitude is approximated to a leading
order as a power-law function of frequency $\nu^{-7/6}$ for the
inspiral phase, followed by $\nu^{-2/3}$ for the merger stage and a
Lorentzian function around the quasi-normal mode ringdown frequency
for the ringdown stage.

For this study, we convert to a energy spectrum to account for the
individual source emissions. We choose two template models: one from
\citet{IMR}, for a non-spinning case, and another from
\citet{spin_IMR} for BBHs with non-precessing spins. In \citet{IMR}
the Fourier amplitude is given by their equation (4.13), which we
convert to an energy spectrum $dE/d\nu$. As we expect the inspiral
spectrum to equal the post-Newtonian approximation \citep[see, e.g.,][]{Cutler93,Finn93}, the inspiral-merger-ringdown spectrum for
a BBH with component masses $m_1$ and $m_2$ is given by

\begin{equation}
\label{dedf}
 \frac{dE}{d\nu} \equiv \frac{(G \pi)^{2/3} M_c^{5/3}}{3}
\left\{\begin{array}{l}
\displaystyle \nu^{-1/3} \hspace{3mm} \mathrm{if}\, \nu < \nu_{1} \\\\
\displaystyle \omega_1 \nu^{2/3} \hspace{3mm} \mathrm{if}\, \nu_{1} \leq \nu < \nu_{2} \\\\
\displaystyle \omega_2 \left[ \frac{\nu}{1+(\frac{\nu-\nu_{2}}{\sigma/2})^2} \right]^{2}\, \hspace{2mm} \mathrm{if}\, \nu_{2} \leq \nu < \nu_{3} \\
\end{array}
 \right.
\end{equation}

Here $M_c$ is the chirp mass, $M_c^{5/3}=m_1 m_2 (m_1+m_2)^{-1/3}$,
$\omega_1=\nu_{1}^{-1}$ and $\omega_2=\nu_{1}^{-1} \nu_{2}^{-4/3}$
are constants chosen to make $dE/d\nu$ continuous across $\nu_{1}$
and $\nu_{2}$. The set of parameters ($\nu_{1}, \nu_{2}, \sigma,
\nu_{3}$) can be determined by the two physical parameters (the
total mass $M$ and the symmetric mass ratio $\eta$) in terms of $(a
\eta^2 + b \eta + c)/\pi M$, with coefficients $a, b, c$ given in
Table 1 of \citet{IMR}, producing (404, 807, 237, 1153)\,Hz for a
$10 M_{\odot}\hspace{-1mm}-\hspace{-1mm}10 M_{\odot}$ BBH ($M_c=8.7
M_{\odot}$).

The waveform presented in \citet{spin_IMR}, includes spin effects
through a single spin parameter $\chi = (1+\delta) \chi_{1}/2 +
(1-\delta) \chi_{2}/2$, with $\delta=(m_1-m_2)/M$ and
$\chi_{i}=S_{i}/m_{i}^2$. The parameter $S_{i}$ represents the spin
angular momentum of the $i$th black hole. The corresponding Fourier
amplitude includes a minor correction (related to $\chi$ and $\eta$)
for non-spinning BBHs. We construct energy spectra for BBHs with
non-precessing spins based on their \mbox{equation (1).}

Figure 2 shows the GW energy spectra for a $10
M_{\odot}\hspace{-1mm}-\hspace{-1mm}10 M_{\odot}$ BBH assuming: the
non-spinning case; $\chi=0.85$; $\chi=0$ and $\chi=-0.85$. The two
extreme values for $\chi$ are set by the numerical simulations of
\citet{spin_IMR}, corresponding to both binary components having
maximal spins aligned or anti-aligned with the orbital angular
momentum. The radiation efficiencies for these energy spectra are
$6.7\%$, $9.74\%$, $5.15\%$ and $4.28\%$ respectively. We note that
the radiated GW energy mainly depends on $M_c$ and $\chi$, and that
the energy spectra for $\nu  \lesssim $ 100 Hz show little
variation. We note that effect of orbital eccentricity is not
considered in our derivation of energy spectrum. This has little
effect on our results as the orbits of coalescing compact objects are expected to circularise \citep{circle} before their GW signals reach the sensitive frequency band of ground-based interferometric detectors \citep{eccen}.

\section{The stochastic GW background}
In this section we evaluate the spectral properties of the BBH
background. It is customary to characterize the SGWB by the energy
density parameter

\begin{equation}
\Omega_{\rm{GW}}(\nu_{\rm{obs}})=\frac{1}{\rho_{c}}\frac{d\rho_{\mathrm{GW}}}{d\ln\nu_{\rm{obs}}},
\end{equation}

\noindent where $\rho_{\rm{GW}}$ is the GW energy density, $\nu_{\rm{obs}}$ is
the observed GW frequency and $\rho_{c}=3H_{0}^{2}/8\pi G$ is the
present value of critical energy density required to close the Universe. For a
SGWB of astrophysical origin, $\Omega_{\rm{GW}}$ is related to the
spectral energy density $F_{\nu}$ (in $\rm{erg}\hspace{0.5mm}
\rm{cm}^{-2}\hspace{0.5mm} \rm{Hz}^{-1}\hspace{0.5mm} s^{-1}$) by

\begin{equation}
\Omega_{\rm{GW}}(\nu_{\rm{obs}})=\frac{\nu_{\rm{obs}}}{c^{3}\rho_{c}}F_{\nu}(\nu_{\rm{obs}})
\label{agwb},
\end{equation}

\noindent where $F_{\nu}$ at the observed frequency $\nu_{\rm{obs}}$ can be
written as

\begin{equation}
F_{\nu}(\nu_{\rm{obs}})=\int_{0}^{z_{\rm{sup}}}
f_{\nu}(\nu_{\rm{obs}},z) \frac{dR}{dz}(z) dz \label{fnu},
\end{equation}

\noindent Here, $z_{\rm{sup}}=
\rm{min}(z_{\rm{max}},\nu_{\rm{max}}/\nu_{\rm{obs}}-1)$, with
$z_{\rm{max}}$ the maximum redshift of SFR model and
$\nu_{\rm{max}}$ the maximal emitting GW frequency. The differential
GW event rate, $dR/dz$, is given by equation (1) and $f_{\nu}$ is
the energy flux per unit frequency emitted by a source at a
luminosity distance $d_{L}(z)$

\begin{equation}
f_{\nu}(\nu_{\rm{obs}},z)=\frac{1}{4 \pi d_{L}(z)^{2}}
\frac{dE}{d\nu}(1+z) \label{flux},
\end{equation}

\noindent where $dE/{d\nu}$ is the gravitational energy spectrum
given by equation (5) and $\nu$ is the frequency in the source frame
which is related to the observed frequency by
$\nu=\nu_{\rm{obs}}(1+z)$.

Figure 3 shows the energy density parameter $\Omega_{\rm{GW}}$ of
the BBH background corresponding to five models outlined in Table 1.
The final model (e) approximates the common power-law behavior of
models (a-d) before reaching a peak of $\sim 10^{-9}$ at 400-600 Hz,
and uses a conservative estimate to account for effects of spin, SFR
and delay time. This model is given by $\Omega_{\rm{GW}}
(\nu_{\rm{obs}}) = 1.95 \times 10^{-11} \nu_{\rm{obs}}^{2/3}$ for 1
Hz$< \nu_{\rm{obs}} <$ 400 Hz. We note that using the two extreme
spectra ($\chi=0.85$ and $\chi=-0.85$) in Figure 2 leads to a
variation in the results of less than $40\%$.

\begin{table}
\begin{center}
\begin{tabular}{llcc}
  Model        & source spectrum     & SFR model & Delay time, $t_0$ (Myr) \\
  \hline
  \hline
  a            & non-spinning    & HB06      & $100$  \\
  b            & $\chi=0$        & HB06      & $100$\\
  c            & non-spinning    & HB06      & $500$ \\
  d            & non-spinning    & W08       & $100$  \\
  e            & power law model &           &  \\
  \hline
  \hline
\end{tabular}
\end{center}
  \vspace{-5mm}
  \caption{The 5 models and their parameters used to determine the energy density parameter $\Omega_{\rm{GW}}$ of a BBH background. Model e, a power law approximation, is described in the text.}
\end{table}

We see in Figure 3 that effects of spin, SFR and delay time are
insignificant for estimating the BBH background considering all
other uncertainties in sources rates and systems masses. Combining
the equations used to calculate $\Omega_{\rm{GW}}$, we find the BBH
background is sensitive to $r_{0}$ and average value of $M_{c}$
through the relation $\Omega_{\rm{GW}} \propto r_0\ M_c ^{5/3}$. It
is useful to express model (e) in the form:

\begin{equation}
\Omega_{\rm{GW}}(\nu_{\rm{obs}}) \simeq 4.2 \times 10^{-10}
\left(\frac{r_0}{3.1 \times
10^{-2}\,\rm{Mpc}^{-3}\rm{Myr}^{-1}}\right)
\left(\frac{M_c}{8.7\hspace{0.5mm} M_{\odot}}\right) ^{5/3}
\left(\nu_{\rm{obs}} \over {100\hspace{0.5mm} \rm{Hz}}\right) ^{2/3}
\label{gwb-bbh}\,,
\end{equation}

\noindent allowing us investigate the parameter space $(r_0, M_c)$
for a SGWB in the next section. We note that equation (10) is
consistent with equation (10) of \citet{GWB_P}. Considering that the
most sensitive frequency regime of the second and third generation
detectors is within 100--200\,Hz, we further adopt a cutoff
frequency of 400 Hz when applying this function.

\section{Issues of detectability}
A number of laser interferometric GW detectors have reached their
design sensitivities and have been coordinating as a global array.
These include the LIGO\footnote{\url{http://www.ligo.caltech.edu/}}
detectors based at Hanford (H) and Livingston (L) in USA, the
Virgo\footnote{\url{http://www.virgo.infn.it/}} (V) detector in
Italy and the
GEO600\footnote{\url{http://www.geo600.uni-hannover.de}} detector in
Germany. The LIGO and Virgo detectors are undergoing upgrades that
will produce a order of magnitude improvement in sensitivity.
Advanced LIGO is expected to be operational by 2015 and an Advanced
Virgo facility is expected to begin commissioning in 2011. Other
plans for advanced detectors include
LCGT\footnote{\url{http://gw.icrr.u-tokyo.ac.jp/lcgt/}} (the
Large-scale Cryogenic Gravitational-wave Telescope; denoted as C),
an underground detector to be built by the TAMA group in Japan and
LIGO-Australia\footnote{\url{http://www.aigo.org.au/}} (A), a 4km
interferometric detector that would be based in Western Australia.
Third generation detectors have also been proposed, such as ET, with
a target sensitivity 100 times greater than current instruments.

To evaluate the detectability of the BBH background, we consider the
five advanced detectors introduced above (H,L,V,C,A). We take
LIGO-Australia to have the same sensitivity as Advanced LIGO and for
ET adopt ET-B sensitivity from \citet{et-B} as well as the latest
ET-D sensitivity from \citet{et-D}. Design sensitivity
curves\footnote{Data are taken from
http://wwwcascina.virgo.infn.it/advirgo/,
https://dcc.ligo.org/cgi-bin/DocDB/ShowDocument?docid=2974,
http://www.et-gw.eu/etsensitivities and \citet{lcgt}.} for these
detectors are shown in Figure 4.

\subsection{Duty Cycle}
For a SGWB of astrophysical origin, in addition to the energy
density parameter and characteristic frequency, another useful
quantity is the duty cycle ($DC$). This is defined as the ratio of
the typical duration of a single signal to the average time interval
between successive events, e.g.,
\begin{equation}
DC=\int_{0}^{z_{\rm{max}}} \bar{\tau}(z)dR(z) \label{duty},
\end{equation}

\noindent where $dR(z)$ is the differential event rate given by
equation (\ref{dR}) and $z_{\rm{max}}$ corresponds to the redshift
limit of considered SFR models. $\bar{\tau}(z)$ is the average
observed duration of GW signals generated by individual sources at
redshift \emph{z}, given at leading order by

\begin{equation}
\bar{\tau}(z)= \frac{5c^5}{256 \pi^{8/3} G^{5/3}} [(1+z)M_c]^{-5/3}
\nu_{\rm{min}}^{-8/3} \label{duration}.
\end{equation}

\noindent Here, $\nu_{\rm{min}}$ is the lower frequency bound of the
detector, which is set by the low-frequency seismic ``wall" for
ground-based interferometric GW detectors. The present LIGO detector
has $\nu_{\rm{min}} \simeq 40$ Hz, and this can be reduced to 10 Hz
for advanced detectors and 1 Hz for ET \citep[see][for
details]{Regimbau09}.

In general, a GW background with a $DC$ of unity or above is defined
as continuous\footnote{We note that to allow for a small number of
events that may be resolved at $DC\sim 1$, some authors consider a
more conservative threshold of $DC\sim 10$ to indicate the
continuous regime \citep{Regimbau09,Eric2010}.}. And non-continuous
signals can be further categorized into popcorn noise ($0.1\leq DC <
1$) and shot noise ($DC < 0.1$) type. As source rate evolution will
increase out to large cosmological volumes, some studies investigate
how \emph{DC} too increases with $z$
\citep{coward_regimbau_06,Eric2010}. In this study we are concerned
with the value of $DC$ as seen at the detector and thus equation
(\ref{duty}) is interpreted as a total value.

For a background signal produced by a source population with an
average chirp mass $\langle M_{c} \rangle = 8.7 \hspace{0.5mm}
M_{\odot}$, for rates $r_{1}$ and $r_{2}$ we find $DC$ values of
0.01 and 0.2 for advanced detectors. Therefore the signal will most
likely be of the shot noise category (or at most popcorn noise for
the higher rate $r_{2}$). For ET type detectors the signal will be
continuous with $DC$ values of 5.8 and 80.6 for rates $r_{1}$ and
$r_{2}$ respectively.

Although for advanced detectors, the SGWB calculated in this paper
is not continuous (Gaussian) even at the higher rate $r_2$, we note
that \citet{drasco} have found the cross correlation method nearly
optimal for a $DC > 10^{-3}$ over 1-year integration\footnote{We
note however, \citet{drasco} also proposed a new statistic to search
for SGWB with low duty cycles, which is currently being investigated
in the LIGO/Virgo collaboration.}. In the following sections we
therefore consider the cross correlation statistic to assess the
detectability of the estimated BBH background.

\subsection{Cross correlation of detectors}
The optimum detection strategy for continuous GW background signals
is cross-correlating the output of two neighbouring detectors
\citep[see,][]{SNR,Maggiore}. This requires that the detectors are
separated by less than one reduced wavelength, which is about 100 km
for frequencies around 500 Hz where $\Omega _{\mathrm{GW}}(f)$ might
peak. The detectors also need to be sufficiently well separated that
their noise sources are largely uncorrelated. We note that although
this may not be possible for ET, techniques are in development to
remove environmental noise and instrumental correlations
\citep{Fotopoulos:2008yq}.

Under these conditions, assuming Gaussian noise in each detector and
optimal filtering, a filter function chosen to maximize the
signal-to-noise ratio, SNR for two such detectors is given by
\citep[][equation 3.75]{SNR}
\begin{equation}
{\mathrm{SNR}^2} =  {9 H_0^4 \over 50 \pi^4} T \int_0^\infty df \>
{\gamma^2 (f) \Omega_{\rm{GW}}^2(f) \over f^6 P_1(f) P_2(f)}\
\label{SNR},
\end{equation}
Here $\gamma (f)$ is the `overlap reduction function', which
accounts for the separation and relative orientation of the
detectors \citep{gammaf}, and $P_1(f)$ and $P_2(f)$ are the noise
power spectral densities of the detectors, and $T$ is the
integration time. As the optimal filter depends on
$\Omega_{\rm{GW}}(f)$, a range of filter functions based on
theoretical expectations of this function will need to be used.

In this study we use data of relative positions and orientations for
10 independent pairs of the five advanced detectors given in Table 3
of \citet{gamma2} and employ the tensor-mode functions described in
their equations (33-35). For ET we assume two detectors of
triangular shape ($60^{\circ}$ between the two arms) and separated
by an angle of $120^{\circ}$, for which the $\gamma(f)$ has a
constant value of $-3/8$ from 1 Hz to 1000 Hz \citep{Eric2010}. We
adopt a value of SNR = 3 to indicate detection, corresponding with
false alarm rate of 10\% and detection rate of 90\% \citep{SNR}. We
also assume an integration time of 3 years for advanced detectors
and 1 year for ET. \vspace{-2mm}

\subsection{Assessing the detectability using the worldwide network}

Calculating the SNRs for SGWB model (e) shown in Figure 3, we find a
value of 0.14 through cross-correlation by two the Advanced LIGO
detectors H-L. For the other four models shown in Figure 3, we find
variation in SNR of within $20\%$. For ET we find SNRs of 59 and 112
assuming ET-B and ET-D sensitivities respectively for model (e),
indicating that this signal will be easily-detected by third
generation detectors. These results, based on average quantities,
suggest that to detect the BBH background with two Advanced LIGO
detectors will require a rate greater than even the higher rate
estimate, $r_{2}\,\sim 0.43\,\rm{Mpc}^{-3}\rm{Myr}^{-1}$. As there
will exist variation in the sensitivities, locations and
orientations of detectors within a worldwide detector network, it is
useful to compare the performances of different detector pairs and
investigate how combining the network could improve the detection
prospects.

Two approaches of combining 2N detectors to increase the sensitivity
of a stochastic background search have been proposed by \citet{SNR}.
We apply these two methods to a network of 4 second generation
detectors. In each case, the optimal SNR can be expressed as
follows, with individual detectors (1-4) indicated in parenthesis:

(i) \emph{Four-detector correlation} (FC) - can be performed by
directly correlating the outputs of 4 detectors

\begin{equation}
\rm{SNR}^2_{\rm{optI}}\approx {}^{(12)} \rm{SNR}^2\ {}^{(34)}
\rm{SNR}^2 + \ {}^{(13)} \rm{SNR}^2\ {}^{(24)} \rm{SNR}^2 + \
{}^{(14)} \rm{SNR}^2\ {}^{(23)} \rm{SNR}^2\,.
\end{equation}

(ii) \emph{Combining multiple pairs} (CP) - is performed by
correlating the outputs of a pair of detectors, and then combining
measurements from multiple detector pairs
\begin{equation}
\rm{SNR}^2_{\rm{optII}} = {}^{(12)} \rm{SNR}^2 + \ {}^{(13)}
\rm{SNR}^2 + \cdots + \ {}^{(34)} \rm{SNR}^2.
\end{equation}

\noindent We now investigate the detectability of the BBH background
by considering both these two approaches, as well as the
cross-correlation method between two detectors. To do this, we
substitute equation (\ref{gwb-bbh}) for $\Omega_{\rm{GW}}$ into
equation (\ref{SNR}). Although there are uncertainties in $r_0$ and
the true ranges of $M_c$, this approximation allows us to quantify
the advantages of the different approaches outlined above. The goal
here is to provide insight into both the requirements for a
detection and the constraints that can be supported by a
null-detection.

Firstly, we set $M_{\rm{c}} = 8.7 \hspace{0.5mm} M_{\odot}$ and
compare standard cross-correlation measurements between different
pairs of the five advanced detectors (H,L,V,C,A). We also determine
any improvements that can be gained from the two approaches
described above -- (i) FC and (ii) CP. We assess performance through
the values of $r_0$ required to produce a SNR=3.

\begin{table}
\caption {Minimum values of the coalescence rate $r_0$ (in
$\rm{Mpc}^{-3} \hspace{0.5mm} \rm{Myr}^{-1}$) to detect the SGWB
from coalescing BBHs assuming an average chirp mass $M_c = 8.7
\hspace{0.5mm} M_{\odot}$. We explore the result from cross
correlation measurements between different pairs of the worldwide
network of second-generation ground-based detectors (H,L,V,C,A) and
for two approaches of combining 4 detectors (FC and CP), taking a
SNR of 3 indicate detection.}
\begin{center}
\begin{tabular}{lccccc}
\hline \hline
 Pair & A-C & A-H & A-L & A-V & C-H \\
      & 1.88 & 0.90 & 0.85 & 2.31 & 3.11 \\
\hline
 Pair & C-L & C-V & H-L & H-V & L-V \\
      & 10.86 & 1.04 & 0.55 & 1.83 & 1.52 \\
\hline
 Combination & ACHL & ACHV & ACLV & AHLV & CHLV \\
     FC     & 1.25 & 1.16 & 1.10 & 1.04 & 0.75 \\
     CP     & 0.40 & 0.57 & 0.56 & 0.38 & 0.45 \\
\hline \hline \label{table_rates}
\end{tabular}
\end{center}
\end{table}

Table \ref{table_rates} outlines the constraints on $r_0$ we obtain
through these different approaches for second generation detectors.
We see that variation in the function $\gamma(f)$ between different
detector pairs together with different sensitivity levels, produces
a variation in the values of $r_{0}$ required for detection. Among
the 10 independent pairs of the five advanced detectors, H-L
performs best as indicated by the lowest required value of $r_0$
($0.55 \hspace{1mm}\rm{Mpc}^{-3} \rm{Myr}^{-1}$). We note that these
values are above the higher rate $r_{2}$. For cross-correlation
measurements between two ETs, minimum detectable values of $r_0 \sim
1.34 \times 10^{-3} \hspace{1mm} \rm{Mpc}^{-3}\rm{Myr}^{-1}$ and
$r_0 \sim 7 \times 10^{-4} \hspace{1mm} \rm{Mpc}^{-3}\rm{Myr}^{-1}$
are obtained using ET-B and ET-D sensitivities respectively.

The values presented by Four-detector correlation, FC, suggest that
no considerable advantage can be obtained through this approach.
However, we see that by combining multiple pairs, CP, produces the
most consistent improvement, the best of which comes from the AHLV
combination (around a $40\%$ improvement on H-L). Equation (15)
shows that applying the CP method to the 3 identical arms of ET will
reduce the minimum detectable values of $r_0$ by a factor of
$\sqrt{3}$.

\subsection{The $r_{0}$--$M_{c}$ parameter space of a detectable BBH background}

We now adopt the same methods as employed in the last section to
explore the parameter space of $r_{0}$--$M_{c}$ required for a
detectable BBH background. To allow for uncertainties in $M_{c}$, we
consider a large range of (4--20) $M_{\odot}$. This range includes
most values of $M_{c}$ within the low metallicity ($0.1 Z_{\odot}$)
distribution of \citet{metal}. We note however, that for the more
realistic scenario that accounts for early common envelope mergers
as the stars pass through the Hertzsprung gap, the range is more
constrained, with $M_{c}$ around (4--9) $M_{\odot}$.

Figure 5 shows the $r_{0}$--$M_{c}$ space for three different
detection scenarios: 1) cross correlation of H-L -- the best
performing pair of advanced detectors; 2) AHLV (through CP) -- the
optimal combination of 4 advanced detectors; 3) cross correlation of
two ET type detectors using two possible sensitivities (ET-B and
ET-D). Zones encompassed by the two rates, $r_{1}$ and  $r_{2}$, are
shown by the shaded areas.

The figure further confirms that advanced detectors are not likely
to detect the BBH background at the rate $r_{1}$. Detection would
require the high rate estimate, $r_{2}$ and $M_{c} \gtrsim 10
M_{\odot}$. Such a range for $r_{0}$--$M_{c}$ has been predicted by
\citet{Bulik08} through studies of the two BH-WR systems, NGC300 X-1
and IC10 X-1. A null detection would therefore confirm a lack of
understanding in the binary evolution of such systems based on the
single source models employed in this study.

In regards to detection strategies for SGWB signals, Figure 5 shows
some improvement in detectability through the use of CP. As already
noted in Table \ref{table_rates}, AHLV can improve the detectability
by $40\%$ compared with only two Advanced LIGO detectors (H-L).

For ET, for the entire range of $M_{c}$ the signal would be
comfortably detected at the lower rate $r_{1}$. A detectable
continuous background requires a rate of order $10^{-3} \hspace{1mm}
\rm{Mpc}^{-3}\rm{Myr}^{-1}$ or above. In comparison with ET-B, we
find that a larger parameter space can be probed by ET-D due to an
improved sensitivity at lower frequencies ($< 20$ Hz).

\section{Conclusions}
In this paper we have estimated the potential contribution of a
population of coalescing BBHs to a SGWB signal. We are motivated by
recent observations of BH-WR star systems \citep{Crowther} and by
new estimates in the metallicity abundances of star forming galaxies
\citep{2008MNRAS.391.1117P} that have suggested the rate of BBHs in
field populations may be greater than previously expected. We base
the single source emissions on energy spectra calculated from recent
parameterized waveforms of \citet{IMR,spin_IMR}. Then, assuming that
the BBH rate traces the SFR with some delay time, we derive cosmic
source rate evolution models and extrapolate our single-source model
out to high redshifts. Rather than a population synthesis approach,
we assume average properties (e.g., masses and spins) for the BBH
population to determine the characteristics of the SGWB signal and
principal parameters to which the BBH background is sensitive.

Our results show that for $M_{c} \lesssim 10 M_{\odot}$, the
background is not likely to be detected through cross-correlation by
two advanced detectors even at $r_{2} \sim
0.43\,\rm{Mpc}^{-3}\rm{Myr}^{-1}$. Only for greater values of
$M_{c}$, as have been predicted to result from BH-WR systems such as
NGC300 X-1 and IC10 X-1 \citep{Bulik08}, there is scope for
detection.

To further assess the detection prospects for second generation
detectors, we have considered the possibility of combining a
worldwide network of advanced detectors to improve the
cross-correlation statistic, namely the methods FC and CP described
in section 5.3. We find that of these two approaches, CP can produce
an improvement of up to $40\%$ against a standard cross-correlation
between two detectors. For the third generation detector, ET, the
signal is accessible with a SNR of 59 and 112 at the lower rate
estimate $r_{1} \sim 3.1 \times 10^{-2}\,\rm{Mpc}^{-3}\rm{Myr}^{-1}$
using ET-B and ET-D sensitivities respectively. This signal could
mask the primordial background signal at below around
$\Omega_{\rm{GW}}\sim 4 \times 10^{-10}$ at $\sim 100$\,Hz.

We note that the rates used in this study are computed assuming
Milky Way type galaxies and the standard formation channel --
isolated binary evolution. Massive binary formation in early
elliptical galaxies is expected to improve the coalescence rate
\citep{elli,os10}. This is particularly important for BBHs due to
the longer delay time. In addition, dynamical formation scenarios in
dense stellar environments can make a significant contribution to
BBH rates. These other formation channels will not only increase the
event rate of coalescing BBHs, but also add additional uncertainty
to the average component masses of the BBH population. For example,
simulations by \citet{sado} suggest that the average chirp mass in
clusters is $\langle M_{\rm{c}} \rangle \sim 20 M_{\odot}$, much
larger than the same found in the field $\langle M_{\rm{c}} \rangle
\sim 7 M_{\odot}$. This might indicate two similar backgrounds
peaking at quite different frequencies. We have shown a minimum
detectable $r_0$ for ET at around $10^{-3} \hspace{1mm}
\rm{Mpc}^{-3} \rm{Myr}^{-1}$, which may be in the range of rate
predictions from dynamical formation scenarios
\citep{oleary07,sado,miller}. Therefore, detection at the
sensitivity of ET could enable these two potential background
signals to be untangled, thus allowing the average properties of the
different populations to be probed.

Additionally, clues to how these two populations contribute to a
confusion background may be provided by Advanced LIGO/Virgo through
single detections in the shot noise ($DC \ll 0.1$) regime. New data
analysis techniques, such as the probability event horizon method
\citep{Coward05,Howell07} which extracts the temporal signature from
a population of transient sources or the maximum likelihood
statistic \citep{drasco}, could prove valuable in interrogating this
regime.

In view of future searches for a primordial
background signal, particularly for ET, simulations incorporating
both dynamical and isolated binary formation channels could prove
useful. These will be considered in a future study. \vspace{-2mm}

\section*{Acknowledgments}
We thank Cole Miller for useful discussions during the early stages
of this study. We also thank Luciano Rezzolla for a careful reading
of the initial manuscript and for providing important feedback on
the gravitational wave waveform parameters of coalescing BBHs. The
authors are also grateful to Tomasz Bulik for insightful comments
which have led to some valuable amendments and for providing plots
of chirp mass-delay time relation, to Krzysztof Belczynski and
Michal Dominik for providing the distribution of the BBH delay time
from StarTrack simulations, and to Ilya Mandel for useful discussion
about the BBH parameters. We thank the anonymous referee for useful
suggestions which improved the clarity and presentation of our
results. Z.X.-J. acknowledges the Australian Research Council and
the W.A. Government Center of Excellence Programme for support of
his visit at UWA where this work had been done. Z.Z.-H. is supported
by the National Science Foundation of China under the Distinguished
Young Scholar Grant 10825313 and by the Ministry of Science and
Technology national basic science Programme (Project 973) under
grant No. 2007CB815401.

redpajama_set_name: RedPajamaArXiv


text:
Salish Sea Currents Magazine
Lost freshwater salmon population may still inhabit Lake Washington
Aerial view of kokanee salmon (and a few sockeye) in a Lake Washington tributary. Photo: Jeffrey S. Jensen
By: David B. Williams
Keywords: Species and food webs, Fishes, Freshwater habitat, Salmonids
Scientists think they may have discovered a lost population of native kokanee salmon in Lake Washington. Salmon watchers are monitoring local creeks this fall to confirm the finding.
As a fisheries biologist with the University of Washington, Jeff Jensen was used to seeing salmon in Lake Washington and its tributaries. But in autumn 2017, he saw a type of salmon that surprised him. Jensen was at North Creek, near where he teaches at the UW's Bothell campus, when he noticed what looked to be a run of kokanee, a variety of sockeye that does not migrate to the ocean. He knew that such fish had long been known to inhabit the lake, but he also knew that biologists considered the run to have been extirpated.
Like many species in the region, kokanee exist because of the region's glacial history. Sockeye salmon, which migrate through Puget Sound when young and return to their natal streams to spawn as adults, periodically found their pathways to the ocean blocked by glaciers. When stuck in these lakes, the sockeye adapted to a fully freshwater life (becoming kokanee) and did not revert to their anadromous lifestyle, even after the barrier was gone.
A male kokanee salmon from the Sammamish River. Photo: Craig Barbaccia
Not only were these kokanee biologically unusual, they also tasted different. In her ethnographic study The Puyallup-Nisqually, Marian Smith wrote that the people who lived around the lake "were said to prefer this salmon [kokanee] to that which entered the rivers from the Sound." In addition, by returning to their birth streams late in the year after the run of other salmon species, the kokanee were an important food source for Indigenous people around the lake. Early accounts by settlers and biologists also referenced the kokanee's flavor and abundance.
The local kokanee eventually evolved three distinct groups: a late run still found in a few tributaries in Lake Sammamish and early and middle runs, both of which were thought to no longer exist. (A coalition of groups, in particular the Snoqualmie Tribe, whose people know the fish by its Lushootseed name sʔilas, or "little red fish," are working to restore the Lake Sammamish runs.) Jensen thought that the fish he saw in 2017 could be the middle run kokanee; he also knew that fisheries biologists had made a similar observation in 2011.
Biologists are not certain about what led to the decline of kokanee but habitat loss, pollutants, and the construction of the Lake Washington Ship Canal and Locks are all thought to play a roll. Nor did the kokanee benefit from the introduction of sockeye, Chinook, and steelhead beginning in the 1920s. An additional challenge for biologists was the presence of what they called residual sockeye. The offspring of ocean-going sockeye, they spent their entire lives in fresh water, returning to the spawning grounds as kokanee look-alikes. When Jensen found his kokanee, he wondered if they were these residual sockeye, a new hybrid kokanee/hybrid, or native kokanee that escaped previous observation.
With funding from Trout Unlimited and in collaboration with the Washington Department of Fish and Wildlife Molecular Genetics lab, Jensen ran DNA tests comparing kokanee samples he collected in 2017, along with a subsequent run in 2020, with kokanee and sockeye populations from around the Pacific Northwest. The Lake Washington kokanee were most similar to, but still genetically distinct from, the native Lake Sammamish "late" run kokanee. Jensen's mystery fish appeared to be true native Lake Washington kokanee.
(Because a small chance exists that they aren't, Jensen hopes to run DNA tests on kokanee collected by late 19th-century University of Washington natural science professor Orson Bennett Johnson. Unfortunately, he hasn't been able to obtain usable DNA from the fish, which Johnson collected from a small tributary of Lake Washington in November 1888 and October 1889, or about the same time of year that Jensen first saw his kokanee.)
Dave Kyle, Trout Unlimited, checks a remote site incubator that is used for salmon egg development. Photo: Jeffrey S. Jensen
At present, Jensen has established a network of Salmon Watchers to monitor streams in Lake Washington and lower Sammamish River tributaries. Volunteer citizen scientists select a stream, spend thirty minutes watching for salmon weekly in the fall, and send data on what they see back to Jensen. He has also teamed up with the Three Rivers Chapter of Trout Unlimited to set and monitor fry traps in the spring. To enhance kokanee production, he is planning to deploy two remote site incubators, which are enclosed habitats for salmon egg development.
"It's amazing that, after more than a century of logging, urbanization, and other onslaughts, the native kokanee have been able to hold on as a reminder of the complex ice-age history of Puget Sound and the surrounding freshwater habitats," says Jensen. His hope is that his research, the work being done by other groups, and citizen scientists can further help kokanee to continue their legacy in Lake Washington.
About the author: David B. Williams is a naturalist, author, and educator whose award-winning book Too High and Too Steep: Reshaping Seattle's Topography explores the unprecedented engineering projects that shaped Seattle during the early part of the twentieth century. He is also the author of "Seattle Walks: Discovering History and Nature in the City," "The Street-Smart Naturalist: Field Notes from the City," and co-author of "Waterway: The Story of Seattle's Locks and Ship Canal." His most recent book is "Homewaters: Human and Natural History in Puget Sound" published in 2021 by the University of Washington Press. You can find Williams on Twitter at @geologywriter.
Story licensed under Creative Commons. You are free to copy and redistribute per CC BY-NC-ND 4.0.
Sockeye Salmon (Oncorhynchus nerka)

redpajama_set_name: RedPajamaCommonCrawl


She wants the world to know she's okay.
Between the posts on Instagram and the police incident, many people began speculating about Lindsay's relationship, and some of her close friends were allegedly speaking out in support of her.
The actress eventually deleted that post, but shared a new photo on Instagram yesterday. The picture shows Lindsay on a boat, looking out into the distance. In the caption, Lindsay wrote a long apology to her followers and fans.
Many of the comments on her post have been positive, and fans are reassuring her that they are glad she is okay.


text:
Sears On The Mark
Striker reaches double figures with Gosport brace.
Colchester United striker Freddie Sears reached double figures for the season with his brace against Gosport in the FA Cup on Sunday.
The lively forward has enjoyed his most productive season in U's colours yet and moved to eleven in nineteen games with his penalty and late goal against the non-league side.
He became the 24th U's player to reach double figures within twenty games, and the first since Chris Iwelumo in the 2005/6 promotion season, with Chris getting his 10th goal in the 20th game.
As one of the U's leading all time goalscorers, it is perhaps no surprise that Martyn King wasted no time in reaching double figures in his time with the U's.
In five successive seasons between 1959 and 1964, Martyn hit ten goals in less than twenty games.
His partnership with Bobby Hunt saw them both manage it in 1961/62 and 1962/63, whilst the last time two players managed it in the same season was 1991/92 as Roy McDonough and Steve McGavin grabbed the goals on the way to the U's completing the non-league double.
Here's the list of U's players to have achieved ten or more goals in double quick time:-
1961/62 Martyn King (achieved on 21/09/61)
1969/70 Roy Massey (16/09/69)
1983/84 Tony Adcock (04/10/83)
1959/60 Martyn King (28/09/59)
1970/71 Ray Crawford (21/11/70)
1956/57 Ken Plant (29/09/56)
1976/77 Colin Garwood (16/10/76)
1991/92 Roy McDonough (18/10/91)
1951/52 Vic Keeble (20/10/51)
1961/62 Bobby Hunt (02/10/61)
1965/66 Reg Stratton (16/10/65)
1973/74 Bobby Svarc (24/10/73)
1977/78 Bobby Gough (01/10/77)
1971/72 Brian Lewis (15/10/71)
1991/92 Steve McGavin (30/10/91)
1958/59 Neil Langman (18/10/58)
1981/82 Kevin Bremner (27/10/81)
1950/51 Arthur Turner (11/11/50)
1966/67 Ken Hodgson (12/11/66)
2001/02 Scott McGleish (20/10/2001)
1955/56 Kevin McCurley (05/11/55)
1957/58 Peter Wright (26/10/57)
1981/82 Ian Allison (02/11/81)
1990/91 Mario Walsh (24/11/90)
2014/15 Freddie Sears (09/11/14)
1950/51 Bob Curry (02/12/50)
1993/94 Steve Brown (13/11/93)
2005/06 Chris Iwelumo (19/11/05)


This beautifully crafted Sterling Silver ring features one of the most sacred symbols in Hinduism known as the Devanagari in Sanskrit.
With ties to Buddhism as well this symbol speaks to ones states of conciousness.
In yogi terms Aum is best known for the waking state, the dream state and the state of deep sleep.


Prepare the street to be opened to thousands of people! The Set Up crew helps set up tents, place barricades and signs along the route. This shift takes place before the event.
Help us make Open Streets welcoming and safe for all!


To think that a National chain such as Macy's could have this happen to any customer has left me baffled. We purchased a sectional in November 2008 and almost 8 months later we still are missing a section of our couch. This would irritate many consumers however, we held on for the ride and gave our sales representative Tony, benefit of doubt. After 3 'confirmed' deliveries and a dozen false promises over the phone, we decided to directly talk to the Manager. Apparently, the missing piece to our sectional has NOT even been ordered after all these months. Our sales rep has been lying to us for the past 8 months! Unblievable. We will NEVER buy with Macy's again after being ridiculed and lied to. Talk about Professionalism!


Budweiser and its local distributor, Quality Brands of the Black Hills are proud to be the official beer sponsor of the 75th Annual Sturgis Motorcycle Rally.
It Ain't Necessarily So: Investigating the Truth of the Biblical Past (Charnwood library) [matthew sturgis, John McCarthy] on Amazon.com. *FREE* shipping on qualifying offers.
Carrington Joshua Sturgis, 24, pleaded not guilty but agreed not to challenge the state's version of the facts to one count of possession of a controlled dangerous substance. A trooper from the Maryla.
Population of Gainsborough At the time of the 2006 statcan census, Gainsborough had a population of 250 people. The population of Gainsborough represents 0.03% of the total population of Saskatchewan (which had 985,386 people at that time), making it Saskatchewan's 223rd most populous community.Fife Lake travel The business editor of The Scotsman and Scotland on Sunday newspapers has been found guilty of stalking a female PR consultant. Terry Murden, 57, had previously been in a relationship with Nicki Sturz.
Editor's Note: We asked Sturgis Charter School's Jeffrey S. Hyer to ask a couple of his students to write a feature for CapeCodToday.com about their experiences commuting to school using a Public Tran.
Facts about Alsask Hotels in Englefeld Neidpath weather Neidpath, Saskatchewan 7 Day Weather Forecast – The Weather . – Neidpath, Saskatchewan Weather. Updated on Wed Jul 4 3:45 AM. . SAVED TO MY LOCATIONS. 11. C. feels like9. overcast. top STORY Tornado.When her children were older, she returned to work as a receptionist at the Westfort Hotel. Never one to sit around . Bonnie Bohay (Don) of Englefeld, Sask.; Tim of Thunder Bay and Kerry (Jenny) of .This article states that the number of polar bears in parts of Alaska dropped 40 percent since the late 1990s. 11 years an.
After suddenly pulling out of the Sturgis Music Festival 2004 in mid festival and forcing. Continues Mr. Petschler,"Mr. Rose declines to mention certain facts. He was solely responsible for the mar.
Sturgis | Etsy – XL, X Large, Sturgis, Biker, Cool, Unique, Vintage Inspired, Mens, Womens, Unisex, Tshirt. Lot of 4 unused Sturgis South Dakota annual black hills motorcycles Rally 2005-07 Sew or.. Did you scroll all this way to get facts about sturgis?
Mt Rushmore is the shrine of democracy and located in the Black Hills of SD!
The Chronicles of Downton Abbey: A New Era [Jessica Fellowes, Matthew Sturgis, Julian Fellowes] on Amazon.com. *FREE* shipping on qualifying offers. The Great War has ended, but Downton Abbey is far from peaceful.
Sturgis didn't invent the pretzel. In fact, soft pretzels have been around for more than 1,400 years after being invented by European monks. However, until the.
In August, the group had a presence at the Sturgis Buffalo Chip, a huge annual motorcycle rally. "You can check sources an.


Japan offers many mountainous regions with around 500 places to snowboard ranging from enormous resorts to very small hills, so choice is amazing. The easiest choices are the most popular and they are popular because they are really very good. Not only that, these top resorts speak English which is very helpful for the overseas boarder. Relatively new in the snowboarding arena having only commenced in the 90's, every resort has been planned with precision to excite the snowboarders and provide an impressive level of service. Those visiting the slopes, whether to one of the mega resorts or a smaller beginner area, the culture of Japan is evident offering a unique blend of the old rituals including quaint buildings and hot springs mixed with a modern up-to-date resort experience.


text:
Homestead edge? Look to top-five finishes in Chase
In the previous two editions of the elimination-style Chase for the Sprint Cup, the champion has turned out to be the driver who won the finale at Homestead-Miami Speedway.
Homestead edge? Look to top-five finishes in Chase In the previous two editions of the elimination-style Chase for the Sprint Cup, the champion has turned out to be the driver who won the finale at Homestead-Miami Speedway. Check out this story on USATODAY.com: http://usat.ly/2frOddm
Jeff Gluck, USA TODAY Sports Published 3:12 p.m. ET Nov. 14, 2016 | Updated 2:10 a.m. ET Nov. 15, 2016
After nine months and 35 races the chase for the Sprint Cup has come down to the final four drivers. USA TODAY Sports
Kyle Busch, right, won the 2015 season finale at Homestead-Miami Speedway to claim his first Sprint Cup championship. Joey Logano, left, finished fourth in that race.(Photo: Peter Casey, Peter Casey-USA TODAY Sports)
AVONDALE, Ariz. — In the previous two editions of the elimination-style Chase for the Sprint Cup, the champion has turned out to be the driver who won the finale at Homestead-Miami Speedway.
That's a side benefit for NASCAR's narrative, but winning the race isn't required. The only criteria for one of the final four drivers becoming a champion is beating the other three — even if they finish 37th and the remaining contenders are 38th, 39th and 40th.
It seems unlikely the champions can keep up their Homestead winning streak forever, especially with drivers like Martin Truex Jr., Brad Keselowski, Denny Hamlin and Kevin Harvick out of the Chase. And then there's Kyle Larson, who might just be the Homestead favorite after he nearly won last year's race thanks to his skills on the high line.
That said, it's still likely a championship would take a top-five finish at the very least. So here's a look at the final four contenders, ranked by their number of top-fives so far in the Chase.
Is there a NASCAR title favorite in the Chase final four?
Kyle Busch has quietly had an incredible Chase. His only finish outside the top 10 is a 30th-place result at Talladega Superspeedway, when he dropped to the back of the field on purpose just to ensure his title hopes survived.
His six top-five finishes have included a pair of runner-up finishes (Dover International Speedway and Phoenix International Raceway on Sunday) and a third-place result at New Hampshire Motor Speedway.
As for his Homestead chances? They're pretty good: He won last year to claim his first Sprint Cup Series championship.
Joey Logano's Chase has been quite impressive — and that's becoming a theme. He has two wins this year in the playoff (Talladega and Phoenix) and also finished second at Texas Motor Speedway and in the Chase opener at Chicagoland Speedway.
This is the same driver who made the final four in the first year of this format and then swept an entire round during last year's playoff before getting eliminated thanks in part to Matt Kenseth's intentional wreck at Martinsville Speedway.
Now Logano has to get it done at Homestead, where he's never won but led 72 laps last year en route to a fourth-place finish.
Jimmie Johnson hasn't had an amazing Chase, but he's done enough to put himself in position. He has two wins — at Charlotte Motor Speedway and Martinsville — but also has four finishes outside the top 10.
If Johnson gets his record-tying seventh championship, it won't be like his previous titles. In most of those, he went to Homestead with the title virtually wrapped up based on the kind of results Busch has been getting this year (lots of top-fives). Johnson never really needed an outstanding finish except for 2010, when he entered Homestead trailing Denny Hamlin — and finished second to win his fifth consecutive title.
But that was also his last top-five at the track, and Johnson has finished ninth there each of the past three years.
Chase race finally delivered on thrills
Carl Edwards hasn't had that great of a Chase, but this format favors being good at the right time over 10 weeks of consistency. And Edwards' second-place finish at Kansas Speedway plus his win at Texas have helped him erase six finishes of 12th or worse in the nine races so far.
That inconsistency has been on display recently. His last four results heading into Homestead are 29th (though that was on purpose at Talladega), 36th, first and 19th.
Can he win Homestead? Absolutely. He has two wins there and finished second in the pressure-packed 2011 finale, when he lost the championship on a tiebreaker to Tony Stewart.
Follow Gluck on Twitter @jeff_gluck
Best of the 2016 Chase for the Sprint Cup
Chase finale: Jimmie Johnson celebrates in Victory Lane after winning the race and his record-tying seventh Sprint Cup championship. Mark J. Rebilas, USA TODAY Sports
Chase finale: Jimmie Johnson celebrates at the start/finish line after winning the Sprint Cup championship. Johnson tied legends Richard Petty and Dale Earnhardt Sr. with his seventh career title. Jasen Vinlove, USA TODAY Sports
Chase finale: Jimmie Johnson hoists a championship flag in celebration after winning the season points title. Mark J. Rebilas, USA TODAY Sports
Chase finale: Jimmie Johnson gets a hug from team owner Rick Hendrick after winning the Sprint Cup championship. Mark J. Rebilas, USA TODAY Sports
Chase finale: Joey Logano, left, narrowly avoids crashing with Carl Edwards late in the race. Logano finished fourth, while the wreck knocked Edwards out of the race and out of championship contention. John David Mercer, USA TODAY Sports
Chase finale: Carl Edwards, left, heads to the infield care center after crashing out of the race. John David Mercer, USA TODAY Sports
Chase finale: Kyle Busch heads into a turn during the Ford EcoBoost 400. Busch came up short in his bid for back-to-back championships and finished sixth. Jasen Vinlove, USA TODAY Sports
Round 3: Joey Logano, center, celebrates with his crew after winning at Phoenix International Raceway on Nov. 13 and securing an automatic berth for the championship race. Jerome Miron, USA TODAY Sports
Round 3: Matt Kenseth goes careening into the wall while racing for the lead with Alex Bowman during the first overtime restart at Phoenix. The crash extinguished Kenseth's hopes of racing for his second championship. Christian Petersen, Getty Images
Round 3: Two fans take in the Can-Am 500 from a hill atop Phoenix International Raceway on Nov. 13. Sarah Crabill, Getty Images
Round 3: Carl Edwards, right, celebrates with his crew after being declared the winner of the Chase for the Sprint Cup race at Texas Motor Speedway on Nov. 6. The win clinches a berth in the title race for Edwards. Jerome Miron, USA TODAY Sports
Round 3: Carl Edwards (19) follows Martin Truex Jr. (78) down pit road at Texas Motor Speedway. Edwards bested Truex on their final pit stop to take the race lead before the rain fell again a short time later. Jerome Miron, USA TODAY Sports
Round 3: Safety works help Casey Mears climb from his car after wrecking on the front stretch during the AAA Texas 500 on Nov. 6. Jerome Miron, USA TODAY Sports
Round 3: Jimmie Johnson's daughter Genevieve puts her father's name on the final four column of the Chase for the Sprint Cup leaderboard after Johnson won for the ninth time at Martinsville Speedway to clinch a berth in the title race. Michael Thomas Shroyer, USA TODAY Sports
Round 3: Carl Edwards pulls his car into the garage after hitting the wall at Martinsville. Edwards finished 23 laps down in 36th-place and likely finds himself in a must-win situation in the next two races Chase races. Daniel Shirey, Getty Images
Round 3: Fans in the upper deck of Martinsville Speedway take in the Goody's Fast Relief 500 won by Jimmie Johnson on Oct. 30. Michael Thomas Shroyer, USA TODAY Sports
Round 2: Joey Logano climbs from the roof of his No. 22 Ford to celebrate his win in the elimination race at Talladega Superspeedway on Oct. 23. Glenn Andrews, USA TODAY Sports
Round 2: Brad Keselowski drives to the garage as flames engulf his No. 2 Ford Sunday at Talladega Superspeedway. Keselowski finished 38th and was eliminated from the Chase. Randy Sartin, USA TODAY Sports
Round 2: Smoke pours out of Martin Truex Jr.'s No. 78 Toyota on Lap 41 of the Hellmann's 500. Truex finished last with an engine failure and was eliminated from the Chase. Marvin Gentry, USA TODAY Sports
Round 2: Kevin Harvick puts his name in the third round of the Chase for the Sprint Cup after winning the Hollywood Casino 400 at Kansas Speedway. Jeffrey Becker, USA TODAY Sports
Round 2: Brad Keselowski drives his mangled No. 2 Ford down pit road after spinning into the grass, Oct. 16 at Kansas Speedway. Keselowski finished 38th and dropped to 11th in the Chase for the Sprint Cup standings. Chris Trotman, Getty Images
Round 2: The crew of Chase Elliott changes tires and refuels the No. 24 Chevrolet after Elliott was forced to make a green-flag pit stop because of a left-rear tire rub. Elliott finished 31st at Kansas Speedway and dropped to 12th in the standings. Jason Hanna, Getty Images
Round 2: Jimmie Johnson snaps the longest losing streak in his career - at 24 races - with a victory Oct. 9 at Charlotte Motor Speedway. Peter Casey, USA TODAY Sports
Round 2: Austin Dillon is bumped onto the grass by Martin Truex Jr. during a restart at Charlotte Motor Speedway on Oct. 9. Sarah Crabill, Getty Images
Round 2: Kevin Harvick (4) and Alex Bowman (88) lead the field to green at Charlotte Motor Speedway on Oct. 9. Mike McCarn, AP
Round 1: Martin Truex Jr. holds the checkered flag as he does a burnout after winning Oct. 2 at Dover International Speedway. Mel Evans, AP
Round 1: Jamie McMurray's crew tries to diagnose a mechanical issue in the No. 1 Chevrolet on pit road at Dover. McMurray finished last and was eliminated from the Chase. Chris Trotman, Getty Images
Round 1: Kyle Larson receives a black flag after incurring a penalty for too many men over the wall during a pit stop at Dover. Larson finished six laps down and was eliminated from the Chase. Jerome Miron, USA TODAY Sports
Round 1: Kevin Harvick does a burnout in front of his crew after wining at New Hampshire Motor Speedway on Sept. 25 and securing a berth in the second round. Brian Fluharty, USA TODAY Sports
Round 1: Cars race around the 1-mile oval at New Hampshire Motor Speedway on Sept. 25. Brian Fluharty, USA TODAY Sports
Round 1: Jimmie Johnson leaves the pits after refueling at New Hampshire. Johnson finished eighth. Jim Cole, AP
Round 1: Martin Truex Jr., center, celebrates with his crew and girlfriend Sherry Pollex, holding a phone, after winning the opening race of the Chase at Chicagoland Speedway and securing a berth in the second round. Mike DiNovo, USA TODAY Sports
Round 1: Brian Scott spins out in Turn 4 at Chicagoland Speedway on Sept. 18. Mike DiNovo, USA TODAY Sports
Round 1: Fans sign the start-finish line before the opening race of the Chase, Sept. 18 at Chicagoland Speedway. Robert Laberge, Getty Images


Looking for a dumpster rental corporation may be irritating at times. If you're in Carlton, MN, and are in need of a dumpster, your first phone call should be to 888-279-5557. Utilizing a dumpster rental organization in your area, such as 1 Stop Dumpster Rental, will make the chore of discarding waste less tedious. If you're looking to rent an effective dumpster for a great price, you came to the right spot.
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There are several selections available for a dumpster rental corporation in Carlton, MN. Customer satisfaction is one of the most important aspects of any dumpster rental corporation. Thankfully, when you use 1 Stop Dumpster Rental, you can rest assured that you will be in great hands.
Great customer support comes hand in hand with using a local dumpster rental company. Using a national supplier with a big brand will have descent rates, but will not provide customized service. Renting a dumpster doesn't have to be expensive or difficult, you just have to use the right corporation.
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The polite associates at 1 Stop Dumpster Rental can help you determine the regulations that apply to you. Many types of waste are accepted, but there's some contents that are not allowed. Some of it will depend on where you live. Part of understanding the items you cannot place in a dumpster in Minnesota is something which every customer needs to fully understand.
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Emerson and Repsol have established a strategic alliance to deliver advanced subsurface geophysical technologies to reduce the time to prospect and produce first oil.
Emerson will work collaboratively with Repsol to implement and deploy advanced subsurface imaging technologies, with core technologies developed by Repsol as part of Kaleidoscope, its 10-year innovation project. These advances will be used by a broad range of the geoscience community within Repsol and in all oil and gas companies that choose to license the technologies. The solution combines the latest in high-end visualization, high-performance computing and cloud delivery.
These technologies have contributed to the exploration success ratio of Repsol, with special significance in settings of complex geology in countries like Brazil, Peru and Bolivia.
The partnership, which includes a joint investment of both research and development, will enable Repsol and Emerson to produce commercially available software products for license to help other oil field operators and service companies.
The first phase of the collaboration will provide advanced solutions for velocity determination, including full waveform inversion and advanced solutions for seismic imaging developed in the Repsol Technology Lab. In addition, the collaboration can be extended to a broader range of Repsol subsurface technologies.


Mill Avenue Office L.L.C., an entity owned by GoDaddy founder Bob Parsons, has acquired Hayden Station, a 107,508-square-foot office and retail development in Tempe, for $26.5 million (or $246.49 per square foot). The seller was Holualoa Cos. of Tucson.
Bob Buckley, Tracy Cartledge and Steve Lindley, all senior managing directors with Cassidy Turley's capital markets group, joined Jeff Hartland, Scott Boardman, Trevor Klinkhamer and Brent Mallonee of the firm's office and retail team in arranging the transaction for the buyer and seller.
Formerly known as Hayden Square, the property is located on the southwest corner of Mill Avenue and 3rd Street, near a variety of shopping and dining destinations as well as Arizona State University. It comprises five buildings: 310, 350, 404 and 410 S. Mill Avenue and 51 W. 3rd Street. The four Mill Avenue buildings range in size from 5,642 to 9,548 square feet. The 3rd Street building is a five-story, 74,307 square-foot multi-tenant office building with views of Tempe Town Lake.
The project was 97 percent leased at the time of the sale to such tenants as The Tavern on Mill, Pop Health Man, Logan Simpson Design, NCounter, Mojo Yogurt, Moonshine Whiskey Bar and Downtown Tempe Community, Inc. "Hayden Station has had a history of maintaining high occupancy, even during the recent downturn," observed Stan Shafer, COO of Holualoa Cos.
According to Cassidy Turley, Downtown Tempe is one of the Phoenix metro's strongest office markets. During the first quarter, the Tempe North submarket recorded the lowest overall vacancy in the Valley at 8.4 percent.
The acquisition brings Parsons'holdings in metro Phoenix to more than 760,000 square feet. The firm's local properties include Centerpoint on Mill, Tempe Town Center, Arrowhead Professional Center, Il Palazzo Center, Citadelle Center, The Shoppes at Legacy House, Grayhawk Plaza and McDowell Mountain Marketplace.


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Olivia Blatchford sinks supermum Natalie Grinham
By Alex Wan
Olivia Blatchford (centre) with Amanda Sobhy and coach Paul Assaiante
Olivia Blatchford takes out Dutch veteran
By ALEX WAN – Editor, Squash Mad Asian Bureau
There would be no happy returns for supermom Natalie Grinham after she was denied a place in the main draw of the Naza PSA Women's World Championship by American Olivia Blatchford.
The 38-year-old has been runner-up in the World Championship on four occasions, including one when she lost to Vanessa Atkinson when it was held in Kuala Lumpur in 2004.
This time she lost out 7-11, 9-11, 7-11 to the American No.2 Blatchford in the qualifying finals. Blatchford meets England's Sarah-Jane Perry in the first round.
"Honestly, Natalie is a fantastic player and I really admired her. I watched her over the years and I've always learned from her," said Blatchford.
"She's incredible as well, having two kids and yet coming back to play. I really didn't know how to play her. Everyone I asked said they hadn't played her in years. So I was just trying to deprive her of those angles as she is very creative in her game."
Natalie lost to her sister Rachael in the 2007 world final in Madrid. Rachael, now 39, beat Nicol David to win the 2005 title in Hong Kong. This year the two meet up in what promises to be an engaging first round clash, taking place on the Nicol David court at the Bukit Jalil Centre. It will be Grinham's 20th appearance in the competition, dating back to 1994. What an incredible record!
Mariam Metwally, another rising star from Egypt, was the first through to the main draw after she defeated compatriot Amina Yousry in five sets.
The 19-year-old, ranked 39th in the world, did not have it easy as she fought hard for an 11-13, 11-2, 11-2, 9-11, 11-9 win over the 16-year-old Amina.
It was a superb match between two talented Egyptians which had excellent shot-making and retrieval, and world number 51 Amina struck first blood by taking the first 13-11.Mariam however, came back very strongly to take the second and third sets with identical 11-2 score lines.
Amina, the youngest player in this tournament however levelled by taking the fourth 11-9. In the end however it was Mariam who had a little extra in reserve as she completed the win in 68 minutes.
"I was nervous in the first because she is younger than me and I've never played her before," said Mariam. "Amina also played really, really well. She's one of the best upcoming players in her age group. I was more calmed in the second and third to win 11-2 and that's when I thought I would have it easier.
"I was just too relaxed and I got sleepy. But I kept fighting until the end and I hope to do better in the main draw."
Mariam, who is making the main draw of the world meet for the second time, takes on Malaysian No.2 Delia Arnold on Monday.
On the next court, Mexico's sixth seeded Samantha Teran came through with an easy 11-5, 11-7, 11-8 win over Dutch player Milou van der Heijden. Hong Kong also had a pair of players – Joey Chan and Liu Tsz Ling – both easing into the main draw.
Fifth seeded Coline Aumard also battled from a game down to beat Japan's Misaki Kobayashi 7-11, 11-2, 11-7, 11-8 but seventh seed Fiona Moverley of England was sent packing by New Zealand's Megan Craig. The 23-year-old Craig won 11-7, 13-11, 11-9 and she meets American No.1 Amanda Sobhy in the main draw.
The final qualifying match of the day was another cracker as 18-year-old Nadine Shahin of Egypt produced a top-notch performance to beat second seed Line Hansen of Denmark.
The world No.50 was just too good on the day as she won 10-12, 11-7, 11-7, 11-4 and earn herself a date with England's Jenny Duncalf in the main draw.
"It's the first time I made the main draw of the worlds. I tried two years ago in Egypt but I didn't get through," said an elated Nadine. It's also my first time beating Line. It's really the first for everything and I still can't believe it."
PSA W185 Naza Women's World Championship 2016, Bukit Jalil National Squash Centre, Kuala Lumpur.
First Round:
[1] Laura Massaro (ENG) v [Q] Samantha Teran (MEX)
[14] Joshna Chinappa (IND) v Victoria Lust (ENG)
[15] Delia Arnold (MAS) v [Q] Mariam Metwally (EGY)
[6] Omneya Abdel Kawy (EGY) v Emily Whitlock (ENG)
[7] Amanda Sobhy (USA) v [Q] Megan Craig (NZL)
[9] Nour El Tayeb (EGY) v [Q] Liu Tsz-Ling (HKG)
[12] Joelle King (NZL) v [WC] Low Wee Wern (MAS)
[3] Raneem El Welily (EGY) v Tesni Evans (WAL)
[4] Camille Serme (FRA) v [Q] Joey Chan (HKG)
[13] Sarah-Jane Perry (ENG) v [Q] Olivia Blatchford (USA)
[16] Jenny Duncalf (ENG) v [Q] Nadine Shahin (EGY)
[8] Nouran Gohar (EGY) v [Q] Coline Aumard (FRA)
[5] Nour El Sherbini (EGY) v Donna Urquhart (AUS)
[11] Annie Au (HKG) v Dipika Pallikal (IND)
[10] Alison Waters (ENG) v Heba El Torky (EGY)
[2] Nicol David (MAS) v Rachael Grinham (AUS)
Qualifying finals:
Mariam Metwally (EGY) bt Amina Yousry (EGY) 11-13, 11-2, 11-2, 9-11, 11-9 (68m)
Samantha Teran (MEX) bt Milou van der Heijden (NED) 11-5, 11-7, 11-8 (32m)
Liu Tsz-Ling (HKG) bt Deon Saffery (WAL) 11-6, 11-7, 11-6 (20m)
Joey Chan (HKG) bt Amanda Landers-Murphy (NZL) 5-11, 11-2, 11-5, 11-3 (36m)
Olivia Blatchford (USA) bt Natalie Grinham (NED) 11-7, 11-5, 11-7
Coline Aumard (FRA) bt Misaki Kobayashi (JPN) 7-11, 11-2, 11-7, 11-8
Megan Craig (NZL) bt Fiona Moverley (ENG) 11-7, 13-11, 11-9
Nadine Shahin (EGY) bt Line Hansen (DEN) 10-12, 11-7, 11-7, 11-4
Pictures by ALEX WAN
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Under the conditions of high-temperature melting, carbon with good activity and more remarkable graphitization can be obtained by carburizing. The shape of the graphite is better reflected on the casting, which is beneficial to improve the mechanical properties, reduce the tendency of shrinkage, and improve the processing performance. In the electric furnace smelting, the high-quality molten iron is obtained by carburizing by the low iron content or even the zero amount. In terms of material properties, the large proportion of pig iron used in the past has a lower mechanical properties than the same amount of high scrap.
Therefore, the new process of smelting with a graphite recarburizer is superior to the conventionally large proportion of pig iron in terms of cost and finished product performance. Graphitized recarburizer manufacturers have learned that with the promotion and application of recarburizers, graphitized recarburizers have played a certain role in the production of different castings. Graphite recarburizer is suitable for ball milled cast iron with high product quality and sulfur content. The effect and comprehensive cost of coal quality recarburizer are not cost-effective. The method of increasing the absorption rate of recarburizer in intermediate frequency furnace is what?
1. When selecting a recarburizer, it is better to choose a carbonaceous agent with moderate particle size and high density, preferably a graphitized petroleum coke recarburizer. Because the carbonization agent is denser and the larger the particle size, the more difficult it is to absorb. Compared with the power frequency furnace, the intermediate frequency furnace heats up too fast, and the absorption rate of the petroleum coke recarburizer in the intermediate frequency furnace is lower, in order to achieve the recarburizer. Higher absorption rate, avoiding long-term high temperature oxidation of the recarburizer, the power in the early stage should be small enough to prolong the heating time of the graphitized recarburizer to increase the absorption rate.
2. Further increase the efficiency by mechanical agitation and manual stirring when necessary. Due to the poor mixing ability of the intermediate frequency furnace, it should also assist the appropriate manual mixing. For example, the use of transfer bag pouring iron to promote the dissolution and diffusion of the recarburizer enhances the absorption rate. The specific gravity of the recarburizer is small, and manual agitation can reduce the recarburizer floating on the surface. When it is burnt, the stirring can also reduce the carbonation holding time and shorten the production cycle. However, if the stirring time is too long, the recarburizer will be burned seriously, so the proper feeding process and melting power also play an important role in the absorption of the recarburizer.
3. A reasonable method of joining, can not blindly join in one time. In order to avoid slow smelting and heating time, scrap steel and graphite recarburizer are added in batches during the batching process. The melting time of each batch is about 15 minutes. In the early stage of the chemical, lower power is used to avoid excessive temperature. After burning, it is expected to heat up quickly after the molten iron paste. For example, a total of 100KG of recarburizer should be added, and 50KG+30KG+20KG should be added to avoid the large-scale addition of the recarburizer to the surface of the molten iron. It can not be effectively combined with the molten iron and the temperature is too high to cause burning. The damage is serious, and the amount of the last addition should be relatively small, avoiding the addition of a recarburizing agent to the molten iron in large quantities, resulting in incomplete absorption of graphite recarburizer in the molten iron and production delay.
Steelmaking basically uses coal-based recarburizers. Although the content of fixed carbon is low and sulfur is high, the melting point of coal-based recarburizer is high, the temperature of cast steel is high, and the absorption rate of coal is low. However, the burning loss is small, and the effect is not worse than that of graphitization. In summary, the method of adding the charge is preferably the addition of carbon to the ingredients, and the graphitized recarburizer and the scrap are added in batches at the same time, and the last addition is increased. The amount of carbon should be as small as possible.
In process of recarburizer + scrap steel What should paid attention to ?


Music is the universal language. The simple and obvious reason for this is that is moves us all at our core regardless of the country it originates from. We do not need to learn the language of the composer to hear, understand or feel the rhythm, the beat, the soul message it relates. Of course, there are different types of music and some of us like a particular type more than an another. Within the universal language there is something for everyone.
What exactly does music do for us? On one level it serves as a means of entertainment. On another level, we listen to music simply because we cannot tolerant the silence in our lives. Silence often makes us feel alone and lonely so we listen to music or the television for "noise". On yet another level it enables us to release some physical energy. Sometimes we are full of energy and we need to move. Moving or dancing to music enables us to do this.
On a deeper level however, music touches us at our core. If we are truly attentive to the music we listen to and allow ourselves to enter into its depths, music has the ability to touch our soul. Music, well done, can move us to tears, whether of sorrow or joy. None of this can happen however if the person listening does not allow him/herself to be touched. When we listen to music or actually participate in the playing or singing of music, we need to allow our emotions to be touched. Otherwise nothing will happen. If we go to a concert and do not enter into the music we may find the evening very long indeed.
Church music is a style of music all its own. Nonetheless it is part of the universal language and it certainly has the ability to touch us at our core. Some of the greatest musicians have written beautiful music for church celebrations and that same music continues to be appreciated even in the 21st century.
The Church uses music to help the people have a fuller, deeper experience of the liturgical celebration. Music is that element that allows us to be touched with our entire being. When we sing or listen to the music, we engage in an activity that has the potential to lift us to the heights or depths of our being. We can experience joy, sorrow, pain or elation. We can express love, passion in service, deep gratitude etc.
Why then, is the music at Mass so "dead"? There are many reasons for this. Some people claim they do not have a good singing voice. Some seem to think that the music simply distracts them from praying. Still others think that the music element of the Mass should be performed rather than participated in. And, of course, there are a number of people who see the music as an element of "entertainment" while at Mass. There are those who would like the music to provide a source of energy release, etc. When these things do not happen they become disgruntled.
Is there a middle ground to all this? Like everything else in life, the answer is Yes. Music can be better chosen, better played, better sung. On the flip side, the people attending Mass must be willing to enter the depths of the music that is chosen to express the themes of the weekly celebration. If the theme is sorrow or reconciliation the music must relate to the theme.


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