text:
9 of the best quotes from Quincy Jones' sweeping Vulture interview
Kelcie Willis, Cox Media Group National Content Desk
Music industry icon Quincy Jones was incredibly candid in a wide-ranging interview with Vulture published Wednesday.
The 28-time Grammy award-winner spoke with New York magazine's entertainment and culture website about Michael Jackson, dating Ivanka Trump, the current state of music and who he thinks killed John F. Kennedy, among a number of other topics.
Here are some of the juciest quotes from Jones' chat with Vulture, which was edited and condensed from two conversations.
On Michael Jackson's musicianship: "I hate to get into this publicly, but Michael stole a lot of stuff. He stole a lot of songs. (Donna Summer's) 'State of Independence' and 'Billie Jean.' The notes don't lie, man. He was as Machiavellian as they come.
"Greedy, man. Greedy. 'Don't Stop 'Til You Get Enough' — Greg Phillinganes wrote the C section. Michael should've given him 10 percent of the song. Wouldn't do it."
On The Beatles: "That they were the worst musicians in the world. They were no-playing (expletive). Paul was the worst bass player I ever heard. And Ringo? Don't even talk about it. I remember once we were in the studio with George Martin, and Ringo had taken three hours for a four-bar thing he was trying to fix on a song. He couldn't get it. We said, 'Mate, why don't you get some lager and lime, some shepherd's pie, and take an hour and a half and relax a little bit.' So he did, and we called Ronnie Verrell, a jazz drummer.
"Ronnie came in for 15 minutes and tore it up. Ringo comes back and says, 'George, can you play it back for me one more time?' So George did, and Ringo says, 'That didn't sound so bad.' And I said, "Yeah, (expletive) because it ain't you.' Great guy, though."
On social issues of class, racism and sexism: "The rich aren't doing enough. They don't (expletive) care. I came from the street, and I care about these kids who don't have enough because I feel I'm one of 'em. These other people don't know what it feels like to be poor, so they don't care.
"We're the worst we've ever been, but that's why we're seeing people try and fix it. Feminism: Women are saying they're not going to take it anymore. Racism: People are fighting it. God is pushing the bad in our face to make people fight back."
On allegations against his friend, Bill Cosby, Brett Ratner and Harvey Weinstein: "It was all of them. Brett Ratner. Weinstein. Weinstein — he's a jive (expletive). Wouldn't return my five calls. A bully."
On Donald Trump: "I used to hang out with him. He's a crazy (expletive). Limited mentally — a megalomaniac, narcissistic. I can't stand him. ...
"He doesn't know (expletive). Someone who knows about real leadership wouldn't have as many people against him as he does. He's a (expletive) idiot."
On dating Ivanka Trump 12 years ago: "She had the most beautiful legs I ever saw in my life. Wrong father, though."
On who killed John F. Kennedy: "(Chicago mobster Sam) Giancana. The connection was there between Sinatra and the Mafia and Kennedy. Joe Kennedy — he was a bad man — he came to Frank to have him talk to Giancana about getting votes."
On today's pop music: "It's just loops, beats, rhymes and hooks. What is there for me to learn from that? There ain't no (expletive) songs. The song is the power; the singer is the messenger. The greatest singer in the world cannot save a bad song. I learned that 50 years ago, and it's the single greatest lesson I ever learned as a producer. If you don't have a great song, it doesn't matter what else you put around it."
On current artists creating good music: "Bruno Mars. Chance the Rapper. Kendrick Lamar. I like where Kendrick's mind is. He's grounded. Chance, too. And the Ed Sheeran record is great. Sam Smith — he's so open about being gay. I love it. (Music producer) Mark Ronson is someone who knows how to produce."


text:
Context of the project
Four-phase implementation
Regional synergy
Enhancement phase
Trade name and trade mark
Integration of the ERE 132 into the Reford Gardens
Meet the designers of the ERE 132 Eco Home
Build green, it pays off
Design of the ERE 132 Eco Home
For a healthy home
Clean drinking water
Environmental management of the site
Green superhero
Analyze : The ERE 132 Eco Home is a research lab
The team behind the ERE 132 Eco Home worked tirelessly in the spirit of collaboration. The team prioritized the dissemination of information and transfer of knowledge as well as feedback on lessons learned.
The approach is documented and the promotional component of the project is deployed in such a manner as to arouse the interest of a wide audience: professionals, manufacturers and entrepreneurs in the construction sector, educational institutions, elected officials and policy makers, tourists and the general public. In all matters of eco-construction, you will find in the ERE 132 a place of research, discovery and inspiration.
SEVERAL COLLABORATIONS DURING THE ENHANCEMENT PHASE
Madame Josée Forest of Rimouski, whose mandate it was to spearhead stage 3 of the project for the ERE 132 Eco Home, has coordinated the entire enhancement phase with her firm Imaginature.
A monitoring program in real time for the ERE 132 has been put in place to measure the performance of the building and is being run by the CEGEP of Rimouski. In addition to sustaining the enhancement program, it should help to stimulate research and development in terms of green construction within regional industries as well as to facilitate the transfer of knowledge.
Moreover, available to rent, with or without an overnight stay, the ERE 132 allows visitors to contribute to the monitoring activities by staying in the Eco Home and therefore being able to evaluate the comfort and energy efficiency of a sustainable building that has been built with leading edge technology and coupled with the knowledge and expertise of those involved in eco-construction.
Acting as consultant and specialist in the eco-construction enhancement program, the non-profit organization, Ecohome has been involved in the project, notably in the thematic process focused on sustainable architecture and region expertise in eco-construction.
The Digital Imagery Research and Development Centre (CDRIN) at the CEGEP of Matane has enhanced the process of two digital applications. The first one provides advertising of regional expertise in eco-construction in terms of the creation of products and technologies with low environmental impact. The second application aims to raise awareness among visitors of the impacts of their choices in terms of both construction and lifestyle and the subsequent effects on their environmental footprint.
The firm Tortuga Films of Rimouski has produced a documentary on the construction of the ERE 132 Eco Home. The visitor can experience, through the cinematic process of time-lapse, the construction of the building and watch presentation clips from various business partners.
The visual artist Fernande Forest of Rimouski has produced, in conjunction with her firm Graffi-X Communications, the design and image of the interpretative signage. She has also created the visual identification of the project.
ERE 132 Eco Home
200 Route 132,
Grand-Métis, Québec
G0J 1Z0
info@ere132.com
© 2023 MERE 132 Eco Home - All rights reserved - A website from NitroMedia

redpajama_set_name: RedPajamaCommonCrawl


text:
Giławy (Jezioro Giławskie) – jezioro w Polsce położone w województwie warmińsko-mazurskim, w powiecie szczycieńskim, w gminie Pasym.

Dane
 Powierzchnia - 19,5 ha
 Głębokość maksymalna - 5 m
 Typ - linowo-szczupakowe
 Jezioro otwarte, wypływa z niego ciek do jeziora Krzywek

Opis
Jezioro wąskie i bardzo mocno wydłużone z północy na południe. Wysokie i strome brzegi otoczone polami, kępami lasu, a od północy łąkami.

Pasym (gmina)
Jeziora w powiecie szczycieńskim
Jeziora na Pojezierzu Mazurskim

redpajama_set_name: RedPajamaWikipedia


The airport resealing work was officially completed at the end of July. But we are still awaiting formal approval of the work by CalTrans to indicate that the owner met the terms of the mandated repair order. The inspector who issued the letter last year no longer works at CalTrans. An interim inspector informed us that the airport's status will be reviewed during its annual inspection this month.
Before the prep work began we were in contact with the interim inspector to ask many questions about the repairs and the runway markings to ensure that we were doing it all according to FAA standards.
Here are some before and after photos to show the improvements.
Here you can see yellow markings and damaged aspalt on the runway.
You can see that the shallow and damaged areas of the runway have been filled in and resealed, resulting in a smooth and debris-free surface.
Runway markings were brought up to FAA standards for our type of airport with all white paint.
We will post an update again when we have the results of this year's annual inspection. Until then, fly safe everyone!
Well done, folks. Caltrans staff have been supportive in all my dealings with them, including the new person assigned to the region around Ocean Ridge. Best wishes.


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text:
Charlotte Pride Board of Directors
Daniel Valdez
daniel@charlottepride.org
Pronouns: He/Him/His
Daniel is the Director of North Carolina and Mid-South Operations at the Hispanic Federation. He has more than 10 years in nonprofit management working with organizations like Welcoming America, Crisis Assistance Ministry, the Latin American Coalition and Carolinas CARE Partnership. He is passionate about using his talents and experience to advance the mission of organizations working on systemic changes in an effort to make the world a better place for all. Daniel was born in Acapulco, Mexico and grew up in North Carolina. He holds a B.A. in History and Latin American Studies from the University of North Carolina at Charlotte. Daniel has served on the boards of The Charlotte Lesbian and Gay Fund, The Bruce Iron Camp Fund, and Reel Out Charlotte.
Nan Bangs
nan@charlottepride.org
Pronouns: She/Her/Hers
Nan Bangs is the Director, Safety, Health and Risk Reduction for Collins Aerospace, headquartered in Charlotte. Nan has over 29 years of experience with environment, health and safety. Nan holds a B.S. in Environmental Science from the University of Maine and an MBA from Rensselaer Polytechnic Institute. She is a retired Commander in the U.S. Coast Guard Reserve, a role in which she supported 9/11, Hurricane Katrina recovery efforts and the BP oil spill cleanup activities.
Lee Robertson
lee@charlottepride.org
Lee joined Charlotte Pride in 2017 after serving on its Board of Advisors. Lee is an attorney at Robertson & Associates, where he practices construction and commercial litigation, representing business and contractor clients in all types of disputes. Lee is a lifelong Charlottean who has extensive experience advising nonprofit LGBTQ organizations on matters of policy and governance. Lee is also heavily engaged with the Mecklenburg County Bar, the YMCA of Greater Charlotte, and the Charlotte School of Law Alumni Association. Lee earned his B.A. in History from NC State and his JD from the Charlotte School of Law.
Brisa Ramirez
brisa@charlottepride.org
Brisa is an Analyst at 25 Capital Partners. Her responsibilities include portfolio analytics, investment research, and supporting the firm's capital raising activities. Prior to joining 25 Capital, she worked as an Analyst in the Model Validation group at U.S. Bank. Brisa Graduated Magna Cum Laude with a B.S.B.A. in Finance from the University of North Carolina at Charlotte. Through the duration of her undergraduate studies, she held various leadership roles within student body organizations.
Riley Murray
riley@charlottepride.org
Riley Murray has been with Charlotte Pride in many incarnations for 14 years. She has been married to her wife, Dee, for 11 years. Together, they have four grown children and 11 grandchildren. Riley grew up in Santa Barbara, Calif., as the youngest of 11. She moved to Charlotte in 2005 where she quickly got involved with Charlotte Pride. Her day job is a supply chain manager, and she is passionate about traveling, her dog, and spending time with her family. Riley is one of the most enthusiastic advocates for Charlotte Pride you will ever meet and welcomes the whole community to the table because Pride could not be successful without everyone..
Jerry Yelton
Programs & Development Director
jerry@charlottepride.org
Pronouns: He/Him/His / They/Them/Theirs
Jerry Yelton joined Charlotte Pride in November 2017. Originally from Forest City, N.C., Jerry graduated in 2016 from Appalachian State University with a B.S. in Communication Studies. Jerry is a passionate advocate for intentional, intersectional community organizing and development. Throughout their time in undergraduate studies and in community roles, they have worked with a variety of LGBTQ organizations and programs to develop inclusive, thoughtful community actions. Jerry works actively with the Charlotte community at large to create unique, inventive programs to incorporate all LGBTQ voices, stories, and faces.
Matt Comer
matt@charlottepride.org
Matt Comer joined Charlotte Pride in 2008 and has served in several volunteer and board roles, primarily overseeing the organization's media and marketing efforts. In November 2017, Matt transitioned from his role as a board member to become the organization's Communications Director. Matt is a native of Winston-Salem, N.C., and has nearly two decades of experience in local LGBTQ community advocacy, community organizing, journalism and media/marketing work. Matt attended the University of North Carolina-Greensboro and the University of North Carolina-Charlotte. He has worked or volunteered with several LGBTQ organizations regionally and nationally. From 2007 to 2015, Matt worked as editor of QNotes, the Charlotte-based LGBTQ community newspaper of North Carolina. His writing has appeared in a variety of local and national news outlets. Matt's advocacy work and reporting has been widely cited by community and mainstream news-media, as well as several academic writers.
Nada Merghani
Programs Associate
nada@charlottepride.org
Pronouns: She/Her/Hers / They/Them/Theirs
Nada Merghani is the Programs Associate for Charlotte Pride. In 2015, Nada became the first-ever student in UNC history to simultaneously serve as President of both a Muslim Student Organization (UNCW MSA) and LGBTQ+ student organization (UNCW Pride). They joined Charlotte Pride in November 2019 after culminating over five years of nonprofit, political, student, and grassroots organizing experience by the age of 22 — including work with Ignite NC, Democracy NC, the Queer Mobilization Fund, 100,000 Poets for Change, and the Artivist Collective. Nada is a first-generation immigrant who was born in Sudan and seeks to bring visibility to the experiences of LGBTQ+ immigrants and Muslims. Their advocacy work has been recorded and published in various mainstream media outlets.


More FREE Disney's Muppets Most Wanted Printables!
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More FREE Disney's Muppets Most Wanted Printables!
Here are a few more FREE Disney Muppets Most Wanted printables! You print these out and have hours of fun with the kids and their favorite characters!


text:
\section{Introduction}

Turbulence is thought to be a major actor throughout the lifetime of
protoplanetary disks, by regulating  the mass accretion and angular
momentum transport, planetesimal formation and planet migration,
and mixing processes relevant for gas and grain chemistry
\citep[see, e.g.][]{Henning_2008}.
The magneto-rotational instability \citep[MRI,][]{Balbus+Hawley_1991} is currently the most widely accepted
theory for an origin of the effective turbulent viscosity. The
ionization fraction in the outer disk is sufficient to allow
for MRI to operate, but there may be a ``dead'' laminar zone in the inner ($<$ 10 AU) disk
interior,  efficiently shielded from ionizing
radiation \citep{Gammie_1996}. Its extent depends on a
variety of factors including magnetic field morphology, X-ray activity, abundance of metals,
and dust properties \citep{Ilgner+Nelson_2006}.
The 2D disk models by \citet{Keller+Gail_2004} and \citet{Tscharnuter+Gail_2007}
 show the possible presence of large-scale circulation
\citep{Urpin_1984, Regev+Gitelman_2002}, but such motions would
be suppressed by turbulence on the scale of the disk thickness.
These meridional flows may be artifacts of the 2D-hydrodynamical disk models with fixed $\alpha$ viscosity.
More realistic 3D MHD simulations do not show preferential directions of the large-scale gas-flows
\citep[see e.g.,][]{Flock+etal_2011}

Turbulence may also provide a source of relative velocities
for grain coagulation to occur \citep[e.g.][]{Voelk+etal_1980,Beckwith+etal_2000}.
The interplay between gas and solid particle motion,
would also lead to high local ``dust'' overdensities and
planetesimal formation by gravitational collapse \citep{Johansen+etal_2007,
Johansen+Klahr+Henning_2011}.
The turbulent state may have a strong
impact on the migration efficiency \citep{Papaloizou+Terquem_2006,Oishi+etal_2007,Uribe+etal_2011}.
Finally, models of gas-phase chemistry including surface chemistry on
grains are sensitive to the level of turbulent mixing \citep[e.g.][]{
Ilgner+etal_2004, Ilgner+Nelson_2006,Semenov+Wiebe_2011} which may partially explain the presence
of cold CO in disks \citep{Dartois+etal_2003, Semenov+etal_2006, Aikawa_2007, Hersant+etal_2009}.

Despite this enormous importance of turbulence for disks, even its
magnitude is poorly constrained. Most constraints on the
anomalous viscosity parameter $\alpha$ come from measured accretion rates
onto the star, which is mostly determined by inner disk properties.
\citet{Hueso+Guillot_2005}
have attempted to constrain
the overall value of the $\alpha$ parameter by simulations of the
viscous evolution of disks as a function of time. More recent results
on viscous spreading of dust disks from \citet{Guilloteau+etal_2011}
suggest
$\alpha$ decreases with time, with values less than $0.001$ near 100 AU
after a few Myr.

Direct measurements of the nonthermal gas motions resulting from mesoscopic
scale turbulence remain rare. \citet{Carr+etal_2004} report supersonic
turbulence from CO overtone bands, but lower linewidths for H$_2$O in SVS13, suggesting strong turbulence in the upper
layers of the inner disk. On the other hand, for the outer disk of
\object{DM Tau}, \citet{Dartois+etal_2003} find marginally larger local velocity
dispersion in $^{13}$CO than in $^{12}$CO, suggesting lower levels
of turbulence in the upper layers than in the disk plane. The
derived broadening, 0.07 to 0.14 km.s$^{-1}$, is subsonic, but
its exact value is difficult to assess because of the contribution
of the thermal component. \citet{Pietu+etal_2007} find
similar results for \object{MWC 480} and \object{LkCa 15}. More recently, \citet{Hughes+etal_2011}
have obtained a low value for \object{TW Hya} ($< 0.04$ km.s$^{-1}$), but up to
0.3 km.s$^{-1}$ for the Herbig Ae star \object{HD 163296} from CO J=3-2 observations.

However, although $^{12}$CO is an interesting indicator, because of the significant
opacities of the lower lying transitions, it only probes
a thin upper layer in the disk, where strong
temperature gradients may affect the apparent linewidth. To build a complete
picture of turbulence in disks, it is thus essential to
constrain the turbulence from other (optically thinner) tracers. CO isotopologues and other molecules
like  HCO$^+$ and CN yield typical linewidths around 0.18 km.s$^{-1}$ at 300 AU,
but attributing this to thermal or nonthermal motions remains difficult,
as their thermal width at 30 K is 0.14 km.s$^{-1}$ \citep{Pietu+etal_2007, Chapillon+etal_2012}.
Moreover, current chemical models fail to explain their vertical location in the molecular
layer since CN, CCH or HCN appear to be in a colder molecular layer than predicted
\citep{Henning+etal_2010, Chapillon+etal_2012}.

It is then important to reduce the uncertainty (and possible bias) introduced by the
thermal contribution to the linewidth.
Among molecules detected in disks, only CS is both abundant enough and sufficiently
heavier than the previously cited ones.

We report here on the study of the CS molecule in the DM Tau disk.
Observations are presented in Section \ref{sec:obs}, disk properties are derived
in Section \ref{sec:ana}, and we discuss the results in Section \ref{sec:dis}.

\section{Observations}
\label{sec:obs}
Observations were carried out with the IRAM Plateau de Bure interferometer. We observed
two different transitions of CS, the J=3-2 line at 146.969047 GHz and the J=5-4 line
at 244.935609 GHz.

For the J=3-2 transition, we used the BC configuration (project RB8F).
The B configuration, with baselines
up to 408 m was observed on 18 Mar 2008, while the more compact C configuration was observed
on 15 Nov 2008. Phase noise ranged from $15^\circ$ up to $55^\circ$ on the longest baselines.
Amplitude calibration was done using nearby quasars and led to an rms level of about $5 \%$.
Absolute flux calibration was done using MWC\,349 as a reference.  The
angular resolution is  $1.4''\times 1.0''$. The correlator provides only a limited spectral resolution
with a channel spacing of 0.08 km.s$^{-1}$, but with an effective resolution of 1.59 times
the channel spacing (i.e. 0.126 km.s$^{-1}$) owing to Welch apodization of the Fourier spectrum.
At this resolution, the brightness sensitivity is 8.8 mJy/beam, which corresponds to 0.35 K at this angular
resolution. Channel maps of CS(3-2) obtained after smoothing in velocity
to 0.16 km.s$^{-1}$ are presented in Fig.\ref{fig:cs32}, but our analysis uses the
unsmoothed data.

The CS(5-4) data were obtained on 11 Nov 2004, 17 Nov 2004, and 03 Apr 2005 (Project OA45).
The natural weighting spatial resolution is $2.6'' \times 1.8''$ at PA 85$^\circ$. We smoothed
the data to a spectral resolution of 0.25 km.s$^{-1}$ for the analysis.
The brightness sensitivity is 90 mJy/beam, corresponding to 0.4 K.
The CS(5-4) is barely detected (at the $5 \sigma$ level): a spectrum towards DM Tau obtained at
3.5$''$ resolution is shown in Fig.\ref{fig:cs54}. The data is compatible
with the integrated spectrum obtained with the 30-m by \citet{Dutrey+etal_1997}
and a source size of about 5$''$, with an integrated line flux $\simeq 0.6 \pm 0.1$ Jy.km.s$^{-1}$.

The relative calibration accuracy between the two frequencies is better than 10 \%.
It is based on the precise spectral index of 0.6 for the reference flux calibration source MWC\,349.

\begin{figure*}
   \includegraphics[width=18.0cm]{fig-cs32.eps}
 \caption{Channel maps of the CS J=3-2 emission towards DM Tau.
 The angular resolution is $1.4''\times 1.0''$ and the spectral resolution 0.16 km\,s$^{-1}$.
 Contour spacing is 10 mJy/beam, corresponding to $2 \sigma$ and 0.4 K brightness.
 The cross indicates the position, orientation,
 and aspect ratio of the dust disk.}
  \label{fig:cs32}
\end{figure*}

\begin{figure}
   \includegraphics[width=7.0cm]{cs54-spectrum.eps}
 \caption{Spectrum of CS J=5-4 line towards DM Tau.
 The angular resolution is $3.5''$ and the spectral resolution 0.25 km\,s$^{-1}$.
 The curve is a best-fit Gaussian to emphasize the detection.}
  \label{fig:cs54}
\end{figure}

\section{Results}
\label{sec:ana}

\subsection{Principle of the method}
Line formation in a Keplerian disk is strongly constrained by the velocity gradient
\citep[see, e.g.][in the context of cataclysmic binaries]{Horne+Marsh_1986}.
The line of sight velocity
(in the system rest frame) is
\begin{equation}
V_\mathrm{obs}(r,\theta) = \sqrt{GM_{*}/r} \sin{i}\cos{\theta}
\end{equation}
where $r,\theta$ are the cylindrical coordinates in the disk plane.
The locii of isovelocity are given by
\begin{eqnarray}
r(\theta) &=& ( GM_{*}/V_\mathrm{obs}^2 ) \sin^2{i}\cos^2{\theta} .
\end{eqnarray}
With a finite local linewidth $\Delta v$ (assuming rectangular line shape for simplification), the line at
a given velocity $V_\mathrm{obs}$ originates in  a region included between $r_i(\theta)$ and $r_s(\theta)$ :
\begin{eqnarray}
r_i(\theta) &=& \frac{GM_{*}}{(V_\mathrm{obs}+\Delta v/2)^2}\sin^2{i}\cos^2{\theta} \\
r_s(\theta) &=& \min\left[R_\mathrm{out},\frac{GM_{*}}{(V_\mathrm{obs}-\Delta v/2)^2} .
\sin^2{i}\cos^2{\theta}\right]
\end{eqnarray}
Figure \ref{fig:cinematique} indicates the regions of equal projected velocities for six different values:
$V_\mathrm{obs}>v_d$, $V_\mathrm{obs} = v_d$, $V_\mathrm{obs}<v_d$, and their symmetric counterpart at negative
velocities, where $v_d$
\begin{eqnarray}
v_d &=&  \sqrt{GM_{*} / R_\mathrm{out}} \sin{i} \label{eq:vd}
\end{eqnarray}
is the projected velocity at the outer disk radius $R_\mathrm{out}$.
Figure \ref{fig:cinematique} and Eq.\ref{eq:vd} thus show that the basic shape of the emission as a function
of velocity depends only on inclination $i$, while the stellar mass gives the scaling
factor for the velocity scale. The intensity along the curves given by Eq.\ref{eq:vd} will
depend on the surface density $\Sigma(r)$ and temperature $T(r)$ profiles.  On the  other hand, the spatial spread
perpendicular to this nominal shape depends \textit{only} on the intrinsic linewidth $\Delta v$.
With sufficient angular resolution, we thus expect that $\Delta v$ is only very weakly coupled to any of the
other disk parameters. The angular resolution should be at least high enough to measure
the shape described by Eq.\ref{eq:vd}, i.e., measure the inclination $i$. A more stringent requirement
is to resolve the transverse size perpendicular to the iso-velocity curves. An insufficient
resolution would introduce a coupling between $\Delta v$ and
$\Sigma$ or $T$ as a smaller spatial spread can be compensated for by higher temperature (or opacity) to
lead to the same flux density.

\begin{figure}[!t]
\begin{center}
\resizebox{6.0cm}{!}{\includegraphics[angle=270]{keplerian.eps}} \caption[Cinematique]{\label{fig:cinematique}
Regions of the disk that yield equal projected velocities $v_\mathrm{obs}$. The ellipse is the
projection of the disk's outer edge.}
\end{center}
\end{figure}

\subsection{Simple Model}
\label{sec:ana:power}
To derive quantitative information from the data, we used the radiative transfer code adapted to disk DISKFIT
 \citep[see][for a detailed description]{Pietu+etal_2007}. In a first step (Model A), the CS column densities and rotational excitation
 temperature distributions are parameterized using a power law of the radius:
\begin{equation}
 \Sigma_\mathrm{CS} (r)=\Sigma_0\left(\frac{r}{R_s}\right)^{-p}
 \end{equation}
\begin{equation}
 T(r)=T_0\left(\frac{r}{R_t}\right)^{-q} .
 \end{equation}
As explained by \citet{Pietu+etal_2007}, $T(r)$ is the line excitation temperature, and it is assumed to apply to all
other levels to derive $\Sigma(r)$. We further assume LTE, so that $T(r)$ is now also the kinetic temperature. Then, the
local linewidth consists of a thermal component, plus a turbulent contribution
\begin{equation}
\Delta V(r) = \sqrt{ \frac{2 k T(r)}{\mu m_H} + \delta V_\mathrm{tu}(r)^2 }
\end{equation}
where $\mu = 44$ is the CS molecular weight and $m_H$ the atomic mass unit.
We note that $\Delta V(r)$ is a half width at $1/e$ and
that the full width at half maximum would be 1.66 times larger.
The turbulent component is also parameterized by a power law
\begin{equation}
\delta V_\mathrm{tu} (r) = dV_0 \left(\frac{r}{R_v}\right)^{-e_v} .
\label{eq:width}
\end{equation}
Finally, CS is assumed to be homogeneously distributed in the $z$ direction, with a scale
height given by the disk midplane temperature. The density is given by
\begin{equation}
n_\mathrm{CS} = \frac{\Sigma_\mathrm{CS}}{\sqrt{\pi} H(r)} \exp \left(-(z/H(r))^2\right)
\end{equation}
and the scale height is set to
\begin{equation}
H(r) = H_0 (r/R_h)^{1.25}
\end{equation}
with $H_0 = 16$ AU at $R_h = 100$ AU. This definition leads to a scale height that
is $\sqrt{2}$ times larger than the $H(r)=c_s/\Omega_K$ convention, where $c_s$ is the sound
speed and $\Omega_K$ the Keplerian angular velocity.

All the other geometric disk parameters (systemic velocity, inclination and position angle of the disk
axis) were taken from the analysis of the CO isotopologues performed by \citet{Pietu+etal_2007}.
We also checked that CS gave consistent results with these independent measurements and
that the errorbars on these geometric parameters did not affect the other derived parameters.
A summary of the disk characteristics is given in Table \ref{tab:disk}.

Synthetic images are generated using the radiative transfer code DISKFIT, and model visibilities
computed for each of the observed $u,v$ points. Minimization on the disk free parameters is then
made using a $\chi^2$ criterion based on the difference between the observed and simulated visibilities.
This process avoids the nonlinearities that result from deconvolution.
A modified Levenberg-Marquardt method is used to locate the minima, with multiple restarts
to avoid secondary minima.
The linewidths we are searching for are not very large compared to the effective
correlator resolution (0.126 km.s$^{-1}$, see Section \ref{sec:obs}). Thus, we
simulated the correlator spectral response by oversampling by a factor 4 in velocity space,
i.e., using a velocity sampling bin of 0.02 km.s$^{-1}$,
followed by a convolution with a kernel mimicking the Welch apodization. This kernel
extended over 12 consecutive channels in the oversampled frequency space.

Under these assumptions, the CS(3-2) line emission can be used to constrain
$\Sigma_0,p,T_0,q,dV_0$ and $e_v$. Errobars around the minimum are derived
from the covariance matrix. A proper choice of the pivot values $R_t, R_v, R_s$ must be made to minimize
the errors on the power laws \citep[see][for details]{Pietu+etal_2007}. With our angular resolution
and CS images, $R_t=R_v=R_s = 300$ AU is a good compromise.
A degeneracy occurs between $\Sigma_0$ and $T_0$ if the
line is optically thin (for example, in the high temperature limit, the emission only depends on $\Sigma_0/T_0$), but
this degeneracy is broken if the surface density profile is steep enough to produce an optically
thick core \citep[see][]{Dutrey+etal_2007}. Indeed, from a global fit,
we find $T(r) = (7.2 \pm 0.4) (r/300 \mathrm{AU})^{-0.63\pm0.09} \mathrm{~K}.$
 Assuming this temperature to be the kinetic temperature, we find
an intrinsic \textit{nonthermal} half width at 1/e,
$\delta V_t(r) = 0.13 \pm 0.03 (r/300 \mathrm{AU})^{-0.38 \pm 0.45}$ km.s$^{-1}$.
The outer radius is found to be $540 \pm 10$ AU.

The derived excitation temperature is unlikely to differ much from the kinetic temperature, because
the densities in the disks are substantially higher than the CS(3-2) critical densities, even at the outer radius.
To explain the observed \textit{total} intrinsic width by
thermal motions ($\delta V_\mathrm{th} = \sqrt{2 k T(r) / \mu_\mathrm{CS} m_H} $, with
$\mu_\mathrm{CS} = 44$) would require a high value of $T \simeq 50$ K at 300 AU.
This simple analysis thus indicates that pure thermal motions cannot reproduce the observed emission pattern,
under the assumptions of Model A.

\begin{figure}[!t]
\begin{center}
\includegraphics[width=\columnwidth]{figure-dv-tk.eps} \caption[dvtk]{\label{fig:dvtk}
Derived nonthermal linewidth $dV_0$ at $R_v= 300$ AU as a function of assumed kinetic temperature
profile. $T_0$ is the temperature at $R_t = 300$ AU. The 4 curves correspond
to different exponents $q = 0$ (red), 0.2 (green), 0.4 (blue), and $0.6$ (cyan).
Errorbars are $\pm 1 \sigma$.}
\end{center}
\end{figure}
To strengthen this conclusion,
as our main goal is to constrain $\delta V_t(r)$, we also explored a much wider range
of possible temperature profiles, varying $T_0$ and $q$. Results for $dV_0$ as a function of assumed
$T_0$ are given in Fig.\ref{fig:dvtk} for four values of $q=0, 0.2, 0.4$, and $0.6$. In each case, because the exponent
$e_v$ is not well constrained, we assumed $e_v = q/2$, which corresponds to a constant Mach number.
Figure \ref{fig:dvtk} shows that, unless the kinetic temperature is very high, the nonthermal
linewidth must be $\simeq 0.10 - 0.15$ km.s$^{-1}$ to represent the observations.

\begin{figure}[!t]
\begin{center}
\includegraphics[width=\columnwidth]{figure-flux54-tk.eps} \caption[cs54tk]{\label{fig:cs54tk}
Predicted CS J=5-4 line flux from the best fit models derived from CS J=3-2 observations, as
a function of assumed kinetic temperature profile. The 4 curves corresponding to the different exponents q = 0,
0.2, 0.4, and 0.6 are essentially degenerate. Errorbars are $\pm 1 \sigma$.
The shaded gray area indicates the measured
line flux and its $\pm 1 \sigma$ range. Calibration uncertainty is not included.}
\end{center}
\end{figure}
The CS(3-2) data set itself
suggests low temperatures, but the surface density profile is essentially flat ($p = 0.14 \pm 0.20$), so the constraint
may be considered as relatively weak.  The temperature found  with CS(3-2) is quite compatible
with the one determined from CCH \citep{Henning+etal_2010} and CN and HCN \citep{Chapillon+etal_2012}.
Moreover, the CS(5-4) data, although quite noisy, can be used to rule out high
temperatures. Figure \ref{fig:cs54tk} shows the integrated line flux for the CS(5-4) data using the
best fit parameters found from CS(3-2) as function of $T_0$ and $q$. Clearly,
high temperatures ($> 20$ K) can be ruled out, since they would produce a
much brighter CS(5-4) emission than observed. This is consistent
with the temperature derived from other tracers, although subthermal excitation of the CS(5-4)
in a warmer medium cannot be ruled out.\footnote{This analysis also implicitly assumes a lack of vertical
(excitation) temperature gradient. On one hand, subthermal excitation is less unlikely for the J=5-4
line than for the J=3-2, but on the other,  the J=5-4 has higher opacities, and can thus probe
higher, warmer levels. The balance between the two effects cannot be estimated without
detailed non-LTE radiative transfer models.}

Low temperatures are thus strongly suggested, although not firmly proven, by
this study. In any case, the uncertainties on temperature profile have a negligible
influence on the key parameters of this study, $\delta V_0$, as well as on $p_\mathrm{CS}$.
However, they can affect the derived CS column density by a factor 1.5-2.

\subsection{A more realistic approach ?}
\label{sec:ana:viscous}
The assumption of homogeneous vertical mixing (constant abundance as a function of $z$) is a strong prior.
In practice, chemical models predict that molecules are strongly depleted in the disk plane, owing to the
condensation of volatiles on dust grains.  Thus, the emission of molecules is expected to come from one or
two scale heights above the disk plane. As the scale height is typically 10 \% of the radius, this means the
emission comes from regions inclined $\pm \delta i \simeq 6^\circ$ from the disk midplane.
Because the line of sight velocity is proportional to $\sin (i)$, these two different inclinations result in
a broadening of the projected linewidth, which is not properly reproduced by the assumption of no vertical
abundance gradient. This is essentially as if the emission came from two disks, one inclined by $i+\delta i$
and the other  by $i - \delta i$ along the line of sight \citep[see][]{Semenov+etal_2008}.
To first order, the extra broadening due
to these inclination differences would then be proportional to the rotation velocity, i.e. would decrease as $\sqrt(r)$,
if $\delta i$ is constant. The exponent of the nonthermal linewidth law $e_v$ (see Eq.\ref{eq:width})
derived above is indeed quite close to the Keplerian exponent 0.5 (but with little significance).

In practice, $\delta i$ will vary with radius. On one hand, $h(r)/r$ increases slowly with $r$ (as $\approx r^{0.25}$).
On the other, the height above which molecules are found is expected to decrease in the outer parts of the disk,
because (interstellar or scattered) UV photons can penetrate deeper towards the disk plane. This leads to enhanced
photodesorption, and brings the molecular layer closer to the disk plane. As a consequence, the resulting increase
in inclination spread is smaller in the outer regions than closer to the star. This could also contribute to the
apparent decrease in the nonthermal broadening found previously by our simple analysis.

It is thus essential to check whether nonthermal motions are also required to explain the observations
when CS is confined above the disk midplane.  Although sophisticated chemical models exist, they require a prior
knowledge of the H$_2$ density structure. This density structure is still very uncertain, and parametric chemical
models (which would explore a range of possible solutions) do not yet exist in this respect.

We thus adopted a second parametrization of the CS emission from the disk,  Model B, which
differs from Model A in two ways.  The CS surface density
is no longer a power law.  Instead, the disk surface density (dominated by
molecular hydrogen) follows an exponentially tapered law
\begin{equation}\label{eq:edge}
\Sigma_H(r) = \Sigma_0 \left(\frac{r}{R_0}\right)^{-\gamma}  \exp\left(-(r/R_c)^{2-\gamma}\right) ,
\end{equation}
which is the self-similar solution of the disk evolution when the viscosity is a (time constant) power
law of radius \citep{LindenBell+Pringle_1974}.
CS is then assumed to only be present when the hydrogen column density from the current point
towards the disk exterior (perpendicular to the disk midplane) is lower than some given
threshold, $\Sigma_d$, the \textit{depletion} threshold. In regions where CS exists, we
further assume that its abundance is only a power law of radius.
The disk is assumed to be vertically isothermal. The column density above a given
height $z$ is then given by
\begin{equation}
\Sigma_\infty(r,z) = \int_z^\infty n(r,u) du = \frac{\Sigma(r)}{2} \left(1 - \mathrm{erf} \left(\frac{z}{H(r)}\right) \right) ,
\end{equation}
from which the depletion height $z_d(r)$ can be recovered as a function of $\Sigma_d/\Sigma(r)$
\begin{equation}
z_d(r) = H(r) \, \mathrm{erf}^{-1}\left(1-\frac{2 \Sigma_d}{\Sigma(r)}\right) .
\end{equation}
The CS abundance is therefore given by
\begin{eqnarray}
 X_\mathrm{CS}(r) = & 0 & \mathrm{for~~~~} z < z_d(r) \\
 X_\mathrm{CS}(r) = & X_\mathrm{CS}^0 (r/R_0)^{-p_\mathrm{CS}} & \mathrm{for~~~~} z > z_d(r) .
\end{eqnarray}
In this model, the overall surface density of CS thus follows the law
\begin{equation}
 \Sigma_\mathrm{CS}(r) = X_\mathrm{CS}^0 \left(\frac{r}{R_0}\right)^{-p_\mathrm{CS}} min(\Sigma_d, \Sigma_H(r)) .
\end{equation}

In the modeling, $R_c$ and $\gamma$ are fixed parameters. We used $R_c = 180$ AU and $\gamma = 0.55$,
which were found by \citet{Guilloteau+etal_2011} from high-resolution, dual-frequency continuum, and
$\Sigma_0$ is also taken from this article to obtain  a disk mass of
$0.03 \Msun$, which gives $\Sigma_0(100 \mathrm{AU}) = 9.6\,10^{23}$ cm$^{-2}$ (H$_2$ molecules).

Although imposing the density structure could allow non-LTE modeling to be performed, considering
the large uncertainties on the real density structure\footnote{As stated before, the dust density
distribution in disks (and a fortiori in the
DM Tau disk) is poorly known. For example, the adopted values do not consider the variations in the
dust properties with radius found by \citet{Guilloteau+etal_2011}. \citet{Andrews+etal_2012}
also argue that no simple model represents both the gas and dust distributions in TW Hya.},
CS is assumed to be thermalized because densities are in general high enough, even at one to two scale heights.
The remaining free parameters are now $X_\mathrm{CS}^0$, $p_\mathrm{CS}$,
$T_0$, $q$, $R_\mathrm{out}$, the turbulent width $dV_0$ ($e_V$ being poorly constrained, we used
$e_V = q/2$, a constant Mach number), and the depletion threshold $\Sigma_d$.

Although the rationale for the choice of parameters is based on behaviors predicted by chemical models,
it is important to stress that our approach is still purely parametric. In particular, we make no \textit{a priori} link
between the thermal structure of the disk and the location of molecules.

The optimal value of $\Sigma_d$ was first located through a grid of best-fit solutions computed with $\delta V$
and $\Sigma_d$ and $T_0$ as fixed parameters, and $X_\mathrm{CS}^0$, $p_\mathrm{CS}$ and $R_\mathrm{out}$ as
free parameters. The temperature was set to the best-fit solution found for the power law; similar results were
obtained when allowing the temperature law to vary. This grid search did not
reveal any secondary minimum. We then started from the best fit found in this grid search to proceed with a
global fit
of the parameters, including the temperature law.
The best fit results are presented in Table \ref{tab:disk}. This model provides a slightly better fit to the
CS(3-2) data than the power-law case.

\subsubsection{Turbulent width}
We find a nonthermal component slightly smaller than that derived in the power-law case, but still significant
$dV_0= 0.11\pm 0.015$ km.s$^{-1}$ for $H_0 = 16$ AU.
A lower value is expected, since part of the spatial extent at a given velocity is due to the
spread in inclinations, which is larger in Model B than in Model A (which assumed vertically uniform CS abundances).

\subsubsection{Depletion column density}
The best fit ``depletion'' column density is  $\Sigma_d = 10^{21.7\pm0.1}$ cm$^{-2}$. However,
interpretation of this value is not straightforward. Changing the scale height from 16 AU
(at 100 AU) to 8 or 32 AU does not significantly affect the derived $\Sigma_d$. This indicates that
$\Sigma_d$ is not constrained by the geometry alone. In fact, this value is found because
the CS(3-2) images are apparently better represented by a simple power law for the CS surface density than
by the more complex radial profiles that can  result from the hypotheses made in Model B.  With $\Sigma_d
 \simeq 10^{22}$  cm$^{-2}$ and a power law for the CS abundance, the CS surface density behaves
as a power law (of exponent $p = 0.4 \pm 0.2$) out to $R \approx 400$ AU, close enough to the outer radius of the
CS distribution. With $H_0 = 16$ AU,
model B also leads to slightly higher (but less constrained) temperatures than Model A, around $10\pm2$ K at 300 AU.

\subsubsection{Vertical location}
Although $\Sigma_d$ is mostly constrained by the radial brightness profile in this
case, it does not imply that the vertical distribution is not constrained. Starting from
the best fit of the radial CS distribution, we can actually get an estimate of the system geometry by
treating the scale height as a free parameter. We find $H_0 = 9 \pm 1.5$ (see Table \ref{tab:disk}),
which is consistent with the temperature derived from CS, which indicates $H_0 = 10.4 \pm 1.2$.
The required turbulent width increases when the scale height is diminished.
The depletion height $z_d$ derived from this best fit is plotted in Fig.\ref{fig:deplete}, together
with the corresponding value of $\Sigma_d$. It is important to note that the shape of $z_d$ is
prescribed by our model assumptions. In reality, the distribution of molecules can be substantially
different, but our analysis nevertheless indicates that a substantial fraction of the CS molecules
must reside around one scale height.

\begin{figure}
   \includegraphics[width=\columnwidth]{height.eps}
 \caption{Top: Total
 disk surface
 density $\Sigma(r)$ and column density $\Sigma_d(r)$ above the depletion height
 $z_d(r)$. Middle: Depletion height $z_d(r)$ as a function of radius in the best
 fit model.  The scale height $H(r)$ is also indicated (in red). Bottom: as
 above, but for $z_d(r)/r$ and $H(r)/r$.}
  \label{fig:deplete}
\end{figure}

\subsection{Comparison with chemical models}
\label{sec:ana:chem}

A chemical model for sulfur bearing molecules was developed by \citet{Dutrey+etal_2011}
to explain the integrated line profiles obtained with the IRAM 30-m.
The model predictions were done with the NAUTILUS code \citep{Hersant+etal_2009},
which computes the chemical composition of the gas and interstellar ices
as a function of time. Bimolecular reactions between gas-phase species and
interactions with direct UV photons and cosmic-ray particles, as well as UV
photons induced by cosmic-rays,  are considered, with a network of 4406
reactions for 460 species. Interactions with grain surfaces (including direct
and UV induced dissociations), as well as reactions at the surfaces, through
1773 reactions, determine the abundance of 195 surface species. The NAUTILUS
code is run in the vertical 1D approximation at different radii of the disk
(from 50 to 500 AU). More details on the model parameters and the physical
structure of the disk can be found in \citet{Dutrey+etal_2011}. The
observations of CS presented in this paper have been compared to the Case C for
DM Tau of \citet[][see their Tables 4 and 5]{Dutrey+etal_2011}.

Although this model does not use the same underlying density structure, it is interesting
to compare its predictions to the results derived from the Plateau de Bure data.
Figure \ref{fig:cs-z} shows the distribution of CS molecules and the H$_2$ density and temperature
vertical profiles for several radii.  The range
of heights at which CS is found corresponds to an H$_2$ column density towards
the outside, $\Sigma_\infty(r,z)$ in the range of $10^{22} - 10^{23}$ cm$^{-2}$, except at 50 AU where the
warmer interior leads to enhanced CS abundance at larger depths.

\begin{figure}
   \includegraphics[width=\columnwidth]{tk.eps}
   \includegraphics[width=\columnwidth]{h2.eps}
   \includegraphics[width=\columnwidth]{cs.eps}
 \caption{Predicted distribution of Temperature (top), H$_2$ (middle) and CS (bottom) molecule densities as a function
 of height for several radii: 50 (black), 100 (red), 200 (green),
 300 (blue), and 500 AU (magenta). }
  \label{fig:cs-z}
\end{figure}

The temperature is not the key parameter defining the molecular-rich layer. CS exists
at temperatures well below its evaporation temperature (30 K), as can be seen in
Fig.\ref{fig:cs-z}. The penetration
of UV radiation (scattered from the star and coming from the ISM) is more important in
defining this layer, which is limited by photodesorption near the disk plane and photodestruction
of all molecules near the disk surface. Temperature effects become significant only above 30 K, for which
high CS densities can be reached because of thermal desorption.

The enhanced CS surface density within 50 AU from the star is not probed by our observations, which are mostly
sensitive to the 100 - 500 AU region.  In this region, the predicted column density
increases slightly with radius \citep[see][Fig.4]{Dutrey+etal_2011}, while the analysis of our observations
indicates a roughly constant or slightly
decreasing column density.
The chemical model does not include any radial
or vertical mixing, that would be a natural consequence of the observed turbulent velocities.
Vertical mixing will on average decrease the altitude at which CS molecules
are found, while radial mixing will smooth out the CS \textit{abundance} distribution.
Consequently, radial mixing would tend to make the slope of the CS surface
density profile closer to the one of H$_2$ that is expected to vary roughly as $1/r$.
This smoothing effect due to mixing can be seen in the study of \citet[][see their Fig.11]{Semenov+Wiebe_2011},
who investigated the impact of radial and vertical turbulent mixing. \citet{Semenov+Wiebe_2011} also
find that the CS content can be increased by an order of magnitude by mixing. Higher angular resolutions
(0.1 -- 0.3$''$) with ALMA are required to directly probe the inner disk region and prove (or disprove) our theoretical
prediction of high CS abundance here.

\begin{figure}
   \includegraphics[width=\columnwidth]{cs-vs-sigmad.eps}
 \caption{CS molecule density as a function of (essentially H$_2$) column density for several radii:
 50 (black), 100 (red), 200 (green), 300 (blue), and 500 AU (magenta). }
  \label{fig:cs-sigma}
\end{figure}

The chemical models predict that CS molecules are located between $z/r = 0.2$ and 0.4 (see Fig.\ref{fig:cs-z}), while
our best fit solution indicates $z_d/r \approx 0.15 - 0.2$. When expressed as a function
of $\Sigma_d$, the model predicts the range where CS is abundant reasonably well, a few $10^{22}$ to $\approx
10^{23}$ cm$^{-2}$ as shown by Fig.\ref{fig:cs-sigma}. The small discrepancies suggest that better agreement between
the chemical model and the observations can be obtained by assuming larger dust grains and a geometrically thinner
(i.e. colder) disk in the model. In this case, the molecular layer is expected to become closer to the disk plane
\cite[e.g.][]{Aikawa+Nomura_2006}, because of enhanced UV penetration and lower sticking efficiency.
Dust settling would also bring the molecular layer in the same direction, by minimizing the sticking efficiency
above the disk plane, but should be less important than grain growth since it only concerns the largest grains
that offer less surface area per unit mass.

\section{Discussion}
\label{sec:dis}

The analysis presented above unambiguously  indicates that a substantial additional line
broadening is required besides the thermal component and that the derived
magnitude of the turbulent motions is not too critically dependent on the assumptions
about the location of the CS molecules.

In the simple power-law approach (Model A), using our temperature measurement, a mean molecular
weight $\mu = 2.30$, the derived sound speed is
$ C_s(r) = \sqrt{k T(r)/\mu m_H} = 0.16 (r/300 \mathrm{AU})^{-0.3}\,\mathrm{km.s}^{-1}$
(using the temperature derived from CS for the kinetic
temperature), which corresponds to a Mach number $M = \delta V_t/C_s/\sqrt{2}$ around 0.5 and
a slightly lower value for Model B.

This result contrasts with the expectations from the $\alpha$ prescription
of the viscosity, where the turbulent width is related to $\alpha$ in a way that
depends on the nature of the turbulence. The value of
$\delta V$ ranges between a few $\alpha C_s$ to  $\approx  \sqrt{\alpha} C_s$
\citep{Cuzzi+etal_2001}. All indirect measurements of the $\alpha$ parameter \citep{Hartmann+etal_1998,
Hueso+Guillot_2005, Guilloteau+etal_2011} indicate $\alpha$ values between a few $10^{-4}$
and about 0.01, thus predicting much smaller turbulent widths, of at most
0.04 km.s$^{-1}$ if extrapolated near 300 AU.  However, these measurements often sample smaller
regions. \citet{Hartmann+etal_1998} derive these from accretion rates, and are thus sensitive
to the inner AUs only. The results of \citet{Hueso+Guillot_2005} and \citet{Guilloteau+etal_2011}
are based on viscous spreading of the dust disk, and are mostly sensitive to the 100 AUs range.

\citet{Hughes+etal_2011}
obtained a low value for TW Hya ($< 0.04$ km.s$^{-1}$), but up to
0.3 km.s$^{-1}$ for the Herbig Ae star HD\,163296 from CO J=3-2 observations.
An attractive explanation of these very different turbulence levels could have been
the age difference between these two stars,  with turbulence level decreasing with age as independently suggested
by the \citet{Guilloteau+etal_2011} results. Our DM Tau result does not fit well in this scheme, as DM Tau is
rather old, too. Differences in inclinations between the nearly face-on disk of TW Hya and the more inclined ones
of DM\,Tau and HD\,163296 could also play a role if the turbulence had significant anisotropy. However, shearing box
simulations of MRI induced turbulence by  \citet{Simon+Armitage+Beckwith_2011} show no evidence for such anisotropy.
On the other hand, \citet{Flock+etal_2011} and \citet{Fromang+Nelson_2006} find small anisotropy,
the radial velocity fluctuations being about 1.5 -- 2 times larger than in the azimuthal or vertical directions.

It is tempting to ascribe the difference between the constraints on $\alpha$ (sampling the disk plane)
and our measured turbulence level (sampling 1-2 scale heights) to the stratification of turbulence predicted by
MHD models. \citet{Fromang+Nelson_2006} and \citet{Flock+etal_2011} show that the velocity dispersion increases
quickly with height above two scale heights (with the $c_s/\Omega_K$ definition, i.e. at $\sqrt{2} H(r)$ with our definition).
However, they only reach a Mach number of 0.4 at four scale heights ($3 H(r)$), which appears insufficient to explain
our result.

The discrepancy between the apparent linewidths and the estimates of the viscosity may also point towards
a weakness in our theoretical understanding of the turbulence. The turbulent width measures velocity dispersion,
while the $\alpha$ viscosity measures a transport coefficient. They are
related through the effective mixing length \citep{Prandtl_1925}, which may not be a simple
function of $\alpha$ and $H$, as is usually assumed in the $\alpha$ model. In
other words, the aforementioned relation between the turbulent Mach number and
$\alpha$ may reach its limits in the disk outer parts.
It is worth pointing out that the TW Hya disk is small (outer radius 230 AU), while those of HD\,163296 and DM Tau are
large ($> 600$ AU and 900 AU, respectively). The smaller turbulent width found in TW Hya is consistent with the
idea that viscous spreading is the main driver for the disk size. Measurements of the nonthermal linewidths for
a wider sample of objects with
different disk radii would be important in establishing this potential link.

It is also important to realize that, in all the analysis of the molecular line emission, the so-called
``turbulent'' width is an adjustable parameter that is used to fit deviations from the simple Keplerian
disk model with purely thermal line broadening. Departure from these ideal conditions will affect the
derived ``turbulent'' width. For example, we have explored in Sect.\ref{sec:ana} the impact of the location
of molecules above the disk plane, but other effects can exist. Small deviations from Keplerian rotation,
which are ignored in our analysis, would have no impact on the linewidth for a nearly face-on object like
TW Hya, but could affect more inclined objects like DM Tau ($i=35^\circ$) or HD163296 ($i=45^\circ$). Our
study of the depletion depth in Sect.\ref{sec:ana} suggests that disk warps would, however, need to be quite
significant ($\sim 10^\circ$) before affecting the required turbulent component.

\begin{table}
\caption{Disk parameters and fit results}
\begin{tabular}{lccl}
\hline
\hline
Geometric        & {Adopted} & Fitted  \\
Parameter        & Value     & Value from CS \\
\hline
Distance (pc)    &  140  & \\
PA  ($^\circ$)   & 65    & $65 \pm 2$   \\
$i$ ($^\circ$)   & -35   & $-35 \pm 1$  \\
$V_\mathrm{LSR}$ & 6.08  & $6.08 \pm 0.02$  \\
$V_{100}$ $(\dagger)$        & 2.16  & $2.17 \pm 0.10$ \\
$M_*$ ($\Msun$)    & 0.54  & $0.54 \pm 0.04$  \\
h                & -1.25 &   \\
\hline
Fitted   & \multicolumn{2}{c}{Density Model} \\
Value    & (A) Power Law   &  (B) Tapered Edge & Note\\
\hline
$\chi^2$ & 2468353 & 2468336 \\
\hline
$H_0$ (AU) (a)  & [16] & $9\pm1.5$ & (1)  \\
$T_0$ (K) (b)   & $7.2 \pm 0.4$ &  $8.0 \pm 1.3$  &  \\
$q$  & $0.63 \pm 0.09$ & $0.60 \pm 0.20$ & \\
$\Sigma_\mathrm{CS}$ (cm$^{-2}$) (b) & $5.9 \pm 2.5\,10^{12}$  & -  & (2) \\
$X_{CS}$ (b)    & -  & $4.2 \pm 4.8\,10^{-10}$ & (2) \\
$p_\mathrm{CS}$ & $0.13 \pm 0.20$ & $0.39 \pm 0.18$ &  \\
$\Sigma_d$ (cm$^{-2}$)  &  - & $\approx 10^{21.7 \pm 0.1}$ & (3) \\
$R_\mathrm{out}$ (AU) & $540 \pm 10$ & $> 580$ & \\
$dV_0$ (km.s$^{-1}$) (b) & $0.13 \pm 0.03$ & $0.12 \pm 0.025$ & \\
$e_V$ & $0.38 \pm 0.45$ & [0.3] & (1) \\
\hline
\end{tabular}
\tablefoot{($\dagger$) Rotation velocity (km.s$^{-1}$) at 100 AU, which determines
the stellar mass $M_*$. (a) at 100 AU, (b) at 300 AU. (1) a number between brackets [] indicate a fixed
parameter. (2) Large errorbar due to strong coupling with temperature.
(3) Error bar not symmetric; derivation from covariance matrix inaccurate.}
\label{tab:disk}
\end{table}

\section{Summary}
\label{sec:sum}

Using the IRAM Plateau de Bure interferometer, we imaged the CS (3-2) emission from the disk of DM Tau
at $\sim 1''$ resolution. Although noisy, CS(5-4) data obtained with the 30-m and at 2.5$''$ resolution from
the PdBI preclude temperatures exceeding about 20-30 K. The morphology of the emission indicates a significant
\textit{local} linewidth,  around 0.14 km\,s$^{-1}$ near 300 AU. This result appears robust with respect to
the assumed location of CS molecules above the disk's midplane. While the magnitude of this linewidth is in
agreement with measurements previously obtained by \citet{Pietu+etal_2007} and \citet{Chapillon+etal_2012} from
other molecules like HCO$^+$, CN, HCN or CO isotopologues, the relatively large molecular
weight of CS (44), combined with the temperature estimate and an accurate handling of the spectral
response of the correlator, leaves no doubt here that this local linewidth is
essentially due to a nonthermal (turbulent) component. The magnitude of these turbulent motions corresponds
to a Mach number around 0.3 -- 0.5.

Our data confirm the relatively low temperatures derived from other molecules  such as CN, HCN, and CCH.
\citep{Chapillon+etal_2012,Henning+etal_2010}. They also suggest the CS molecules are located above one
scale height from the
disk plane, in reasonable agreement with predictions from chemical models.

This work shows the potential of CS as a turbulence tracer. No other molecules detected so far
\citep[including the recently reported HC$_3$N,][]{Chapillon+etal_2012b} is both heavy
and abundant enough to provide a more sensitive tracer.  Also, CS offers a number of transitions in
the mm / submm domain, which probe critical densities ranging from a few $10^5$ to several $10^8$ cm$^{-3}$. This,
combined with its expected location in the molecular-rich layer, make this molecule a key probe of physical
conditions in disks. The constraint obtained for the geometric location of CS molecules with respect
to the disk plane, although still difficult to interpret, clearly indicates the potential of ALMA for probing
different depths.

\begin{acknowledgements}
We thank the Plateau de Bure staff for performing the observations.
This work was supported by the National Program PCMI from INSU-CNRS.
DS acknowledges support by the \textit{Deutsche Forschungsgemeinschaft} through
SPP~1385: ``The first ten million years of the solar system - a
planetary materials approach'' (SE 1962/1-2).

\end{acknowledgements}

redpajama_set_name: RedPajamaArXiv


"Bathym aka Bathim" Greek	 Bathin, Marthin. One of the three demons in the service of Fleuretty. Duke of the Infernal regions he has the appearance of a robust man but his body ends in a serpent's tail. He is well versed in the virtues of herbs and precious stones according to Wierius. He is able to transport men from one place to another with wondrous speed. He commands thirty legions. One of the 72 spirits of Solomon.


text:
Physocarpus, commonly called ninebark, is a genus of flowering plants in the family Rosaceae, native to North America (most species) and northeastern Asia (one species).

Description
Physocarpus are deciduous shrubs with peeling bark and alternately arranged leaves. The leaves are palmate with 3 to 7 lobes and often toothed edges. The inflorescence is a cluster of bell-shaped flowers with 5 rounded white or pink petals and many stamens. The fruit is a flat or inflated dehiscent follicle.

Physocarpus opulifolius is cultivated as an ornamental plant. Several cultivars have been bred, particularly for foliage of varying colors, including 'Dart's Gold' and 'Luteus', which have yellowish leaves, and 'Monlo' and 'Seward', which have reddish purple foliage.<ref>[http://urbanext.illinois.edu/ShrubSelector/detail_plant.cfm?PlantID=354 Common Ninebark, Physocarpus opulifolius'.] University of Illinois Extension.</ref>

Taxonomy

 Species
There are sixOh, S. H. and D. Potter. (2005). Molecular phylogenetic systematics and biogeography of tribe Neillieae (Rosaceae) using DNA sequences of cpDNA, rDNA, and LEAFY. American Journal of Botany 92(1), 179-92. to 20 species in the genus. They include:Physocarpus alternans  – dwarf ninebark (western North America)Physocarpus amurensis  – Asian ninebark (Asia)Physocarpus australis Physocarpus bracteatus  – (Colorado)Physocarpus capitatus  – Pacific ninebark (western North America)Physocarpus glabratus  – (Colorado)Physocarpus malvaceus  – mallow ninebark (western North America)Physocarpus monogynus  – mountain ninebark (North America)Physocarpus opulifolius  – common ninebark (eastern North America)Physocarpus pauciflorus Physocarpus ribesifolia  – (Asia)

SynonymsPhysocarpus hanceana  = Neillia hanceana Physocarpus intermedius  = Physocarpus opulifolius var. intermedius
 Physocarpus torreyi  = Physocarpus monogynus Physocarpus stellatus  = Physocarpus opulifolius

 Etymology
The genus name Physocarpus'' comes from the Greek word for "bladder fruit", referring to the inflated fruits of some species. The common name 'ninebark' refers to the peeling bark of mature branches, which comes away in strips.

Cultivation
Propagation is by seeds sown as soon as ripe or they can be stored dry in airtight containers in a cool place for up to a year and then sown. Plants can be divided in the early spring, with a sharp spade or even an axe, chopping right through the middle. Softwood and hardwood cuttings are easy to root.

Garden writers describe few if any problems, but it is not unheard for armies of aphids to attack some varieties. Some seaside specimens exhibit powdery mildew in summer.

References

External links

Neillieae
Rosaceae genera


text:
Schoettella idahoensis är en urinsektsart som först beskrevs av John L. Wray 1958.  Schoettella idahoensis ingår i släktet Schoettella och familjen Hypogastruridae. Inga underarter finns listade i Catalogue of Life.

Källor

Hoppstjärtar
idahoensis


KARACHI: Pakistan Peoples Party (PPP) chairman Bilawal Bhutto Zardari pledged that they will transform Karachi into a city of opportunities for all, according to a press statement issued by the party.
The PPP chairman said so while presiding a meeting of PPP leaders from Karachi division to discuss election strategy in the city.
The meeting was attended by Leader of the Opposition in Senate Sherry Rehman, Rashid Rabbani, Waqar Mehdi, Saeed Ghani, Javed Nagori, Nabeel Gabol, Yousuf Baloch, Najmi Alam, Khalil Hoath, Karamullah Waqasi, Nadya Gabol, Nadir Gabol, Shakeel Chaudhry and others.
Speaking at the meeting, Bilawal said that Karachi had been freed from the clutches of 'Na-Maloom Afrad (unknown individuals)', and due to initiatives and efforts of the last PPP government , peace has been restored in the city to a great extent.
He said that people of Karachi will be exercising their right of franchise for the first time without any coercion and intimidation.
The PPP chairman claimed that his party will sweep general elections in Karachi as it had served the people of the city, who can more easily differentiate between anti-PPP propaganda and the services rendered by his party for the metropolis, despite having lesser mandate from it.
Bilawal further urged the PPP leaders and workers from Karachi to step-up campaign and take the message of the party to every door in the city.


text:
Science Museum in London the venue for Cornwall and West Devon Mining Landscape World Heritage Team exhibit | Cornish Lithium Ltd
24 Mar Science Museum in London the venue for Cornwall and West Devon Mining Landscape World Heritage Team exhibit
Cornish Lithium's directors Derek Linfield (left) and Jeremy Wrathall plan to start Europe's only lithium mine
THE Cornwall and West Devon Mining Landscape World Heritage Team is hoping to inspire future innovation from historical insight when it exhibits at the Science Museum 'Lates' Science and Technology event in London on Wednesday.
The Cornish Mining World Heritage Site team will be presenting at the prestigious national venue for the first time and has invited partners from Cornish Lithium and Camborne School of Mines to share their work with the museum's many visitors.
The Science Museum is collaborating with UNESCO UK for the evening of the museum's popular "Lates" events to showcase how their work contributes to making the world a better place for all. Three other UNESCO World Heritage Sites – Stonehenge, Maritime Greenwich and the Forth Bridge – and other internationally important environmental organisations like the British Antarctic Survey will be among the exhibitors selected to showcase the work they do.
Those attending will be invited to discover how Cornwall and Devon's mining heritage assets help present day geologists chart the earth below us.
Other displays will demonstrate how technology is helping us to confront some of the biggest global challenges facing humanity, demonstrating pioneering solutions to issues including climate change, environmental devastation, and flooding.
Deborah Boden, co-ordinator of the World Heritage Site Office, said: "We're delighted to be offered this critical opportunity by UNESCO UK, to showcase how our history of innovation in mining technology can contribute to the next industrial revolution, and will be highlighting how the Cornish Mining World Heritage Site and partners Cornish Lithium and Camborne School of Mines are working together to promote the contribution that environmentally responsible modern mining can make to sustainable development."
Lucy Crane, exploration geologist at Cornish Lithium, said: "Cornish Lithium are thrilled to be a part of the team representing the Cornwall and West Devon Mining World Heritage Site at the Science Museum 'Lates' event.
"Cornwall and West Devon have a rich mining heritage which has produced vast amounts of various metals over the past few centuries, as well as a wealth of useful historical data. The region is now being re-evaluated with modern exploration techniques for its potential to supply some of the critical metals needed for the battery revolution. Coupled with modern sustainable mining techniques, real opportunities for environmentally-responsible mineral extraction are now being identified within the region."
The event is free but a ticket is needed. Further information can be found at www.sciencemuseum.org.uk/see-and-do/lates


text:
775 Lumière este un asteroid din centura principală, descoperit pe 6 ianuarie 1914, de Joanny Lagrula.

Legături externe

 775 Lumière în JPL Small-Body Database
 775 Lumière în baza de date a Minor Planet Center
 Diagrama orbitei asteroidului 775 Lumière (JPL)

Centura de asteroizi
Obiecte astronomice descoperite în 1914


text:
You are here: Posts > Insights > How is the digital era changing Engineering?
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How is the digital era changing Engineering?
01/02/18 Kieran Wilson - CertRP Manager, Manufacturing & Operations
The way we work is changing. With the invention of computers, software and ever-more advanced technology, we have entered the digital age, where multinational businesses and ordinary people alike use technology to transfer money, conduct deals and go about their daily lives. Last year, foreign and local businesses invested £9.2bn into the technology sector, whilst the digital economy continues to grow at twice the rate of the wider economy.
So what does this mean for engineers- and the engineering sector as a whole? The engineering industry is of vital importance to the UK, contributing a whopping 26% of the UK's GDP, so being able to keep ahead of the curve is of paramount importance. As the engineering industry is characterised by innovation and progression, the digital revolution presents enormous opportunities for businesses and engineers alike and is ultimately transforming engineering jobs globally.
With the advanced capabilities presented to us by technology, we expect engineers to be at the forefront of many new developments in the coming years. Kieran Wilson, Redline's Contract and Interim Senior Consultant specialises in Aerospace, Motorsport, Defence and Automation in R&D and Engineering projects. Kieran discusses four key areas where he expects to see significant change in the digital era in engineering:
The digital sector is perhaps the place where engineering is expected to undergo the biggest changes and have the most impact. The role of the digital engineer is changing at an unprecedented rate, thanks to rapid developments in technology and software. The digital sector is ripe for innovation: with new start-ups exploding in popularity and new inventions and apps able to generate millions of pounds in revenue within months. The digital engineering space has never been more exciting, especially given that there are now engineering jobs that didn't exist even five years ago.
Of particular importance is the development of concepts like the 'Internet of Things' and cloud-based storage: the ability to develop software that will be able to keep up with the rapid changes that are taking place in the industry and usable five years from now has become a vital skill. Likewise, AI has become a huge area of interest, with Hanson Robotics debuting its robot Sophia, the most advanced robot in the world, earlier this year, and revolutionising the way many see artificial intelligence.
The rise of digital technology has the potential to transform the Defence sector over the coming years, with 80% of executives within the industry anticipating that the pace of technological change in Defence is going to increase rapidly over the course of the next three years.
The rise of artificial intelligence will allow big data to be mined to analyse and predict events before they happen, or sense incidents that standard intelligence methods can't sense. Furthermore, the rise of big data also has the potential to help streamline production processes, as well as upgrading the equipment in command and control systems to ensure a faster and more comprehensive ability to predict attacks, and respond quickly and effectively to them. This will undoubtedly give rise to a new generation of digitally controlled weapons systems, IT applications and even devices like drones and sensors, all of which will contribute to an overall 'Cloud' database for rapid information sharing.
Engineers will almost certainly be at the forefront of this shift to a more digital frame of mind, with companies recruiting digitally-savvy software engineers, people who are skilled in IT systems, and especially personnel who will be able to adapt quickly to the changing market and technology.
The aerospace sector is making the most of the new opportunities presented by the surge in digital technology: with a projected growth rate of 5.1% over the next decade, manufacturers are revolutionising their digital manufacturing processes to keep up with demand, streamline production processes and cut down on costs.
Inventions like 3-D printing are now more viable than they've ever been, and engineers are capitalising on this boom to create high-quality prototypes quickly and cheaply; indeed, 3-D printing is especially well-suited to the aerospace industry, which often produces products that are tailored to different clients. Using this new method of printing can reduce material costs, labour costs and create specialised components more efficiently, and quickly, than ever before. Even better, this new demand is creating a need for software and hardware engineers, attracting fresh talent and opening up new areas within the industry.
Bio-engineering
The rapid development of advanced technology is allowing engineers to take massive strides in areas like electronics. Nanotechnology has been making unprecedented breakthroughs. With more advanced software comes the ability to manipulate matter at a molecular level, resulting in inventions like tissue nanotransfection, which reprogrammes skin cells, or tiny chips that can be implanted in the skin which could replace contactless cards. One substance, graphene, can even be used as a molecular electrical conductor, giving electrical engineers the chance to shrink down software- for instance, nanotransmitters- even further.
Nanotechnology is hugely versatile. With the ability to create clear nanoscale films for glass, making it both waterproof and UV-resistant, or develop nanoparticles used as catalysis to boost chemical reactions, nanotechnology can be used across a huge range of industries. The possibilities are limitless, and with every new invention comes the chance to explore an avenue of technology as-yet unopened. As technology develops, nanoengineers will be in more demand than ever.
We are at the cusp of the Fourth Industrial Revolution. Technology is transforming the way in which we work, think and live, and engineers will be at the forefront of these changes, transforming the digital age in everything from manufacturing to robotics.
Engineers exist to solve problems. That need is never going to go away.
At Redline, we like to stay ahead of the curve, and stay informed of the latest developments in engineering, so we can continue to match the freshest talent to the best job opportunities. To find out more about how we can help with your engineering and technology recruitment, please contact Kieran Wilson on 01582 878836 or email KWilson@RedlineGroup.com. Alternatively browse all of our jobs in engineering here.
Cathy Swain awarded Level 3 Certificate in Recruitment Practice by the REC
Graham Cross
Hiring still happening, with IT, Computing & Engineering leading the way
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You want to educate yourself about pest management to ensure you use the most applicable technique. Find out about its life cycle, what it eats, what it likes and doesn't like, and so forth. Once you set all of this information collectively, you may create a plan to remove it from your own home. When battling mice near your own home, try mint. Mint should be planted around your private home's perimeter. This will make the mice discover another house that has less aversive stimuli. If in case you have a rodent downside, try sprinkling mint leaves close to where they're hiding. This may repel the mice if the mint is recent.
If you wish to do away with the ants around your home, sprinkle some borax powder close to your house. This can assist to poison the ants so that they are stopped in their tracks and cannot come again. This will assist to quickly get rid of the ant downside throughout sure seasons of the year. All the time make sure that folks and pets are properly protected from a pesticide. Pesticides can cause severe hurt to dwelling things if precaution shouldn't be used. Due to this fact, guantee that the location you apply the pesticide is freed from people, pets, and even toys and and dishes. Be extra cautious when utilizing a pesticide close to a stream, well, garden, college, or office.
Pests are drawn to drains. Be sure you clean and examine them every month, both by utilizing a snake or liquid drain cleaner. You'll be able to develop quite a build up of debris in your drain which makes a lovely house for pests. Once a flea population has been established, they are often very tough to eradicate. It's essential to get rid of all of the fleas and their eggs from any animals who dwell in the home, and in addition kill any eggs, larvae and fleas from bedding and carpets. Remember the fact that it's vital to interrupt their cycle of life, so do not hesitate to repeat the method multiple times.
Anytime you set brushes round your house, make sure you put them a minimum of one foot away. Bugs that nest in wild brush will enter your property if they are close sufficient. For those who find the brush proper next to your house, the bugs will inevitably discover their method inside. With the intention to be successful at getting rid of a pest, it is essential that you're educated concerning the pest. Know what your pest eats, how lengthy it lives, and what it does and would not like. The more you understand a few pest, the simpler it is to create an efficient plan for eliminating it.
They will additionally feed from crops and drink from an aquarium.
To reduce the amount of mosquitoes around your own home, get rid of any areas where there may be standing water. This is the place mosquitoes lay eggs, and it helps them thrive. Look within the backyard, close to your flowers, etc. for water swimming pools. Seize a number of of the pests which might be infesting your house and use them as a reference as you store for pesticides. This can show you how to discover out what sort of product you need to use. Completely different pesticides are efficient on completely different pests. You'll be able to then ensure you are using the right pest control product.
Unclog any drains which will have clogging points. Pests are drawn to that sort of organic material build up. Even just a minor clog can result in roaches and flies coming into your home. Picking up some sort of liquid de-clogger or a de-clogging snake software will do the trick. Handle the issue straight away. There is a saying that when you see one pest, there are a whole lot extra you don't see. That's why it's worthwhile to maintain the problem instantly, as soon as you would possibly notice it exists. Don't wait and hope the problem will go away, as a result of it's possible that it will only worsen.
In case you are pondering of doing pest management your self, just be sure you carry some of the pests with you while you buy your pesticide. This helps the professionals establish the pest and the merchandise you want. Sure pesticides eliminate sure pests. This lets you get the right poison for the precise pest. When you recycle, that is perhaps something pests discover enticing. It's good to hold your recycling exterior if you happen to can. If you can't do that, make sure to rinse every part that goes into the bins. Seal up your recycling bins to maintain pests away.
Have ants? Use lemons. Ants dislike the scent of lemons. Therefore, begin using lemon-scented merchandise, or actual lemons, to do away with them. Try pouring lemon-scented oil along the sides of the rooms in your house. Use lemon-scented products to wipe up within the kitchen. You will soon discover that ants keep away from you. If in case you have ants, search for boric acid. Boric acid, typically listed as orthoboric acid, is the best pesticide for ants. As well as, many of the baits containing this are secure for use around pets and kids, though you must always fastidiously read all safety labels to make certain.
Look in the garden, near your flowers, and many others. for water swimming pools. Anytime you set brushes round your property, ensure you put them a minimal of 1 foot away.


text:
Q: entity level validator not triggered I've observed that when I'm adding an entity to a collection of another entity, the validator for the second entity is not called.
I expected that adding to a child collection triggers entity level validation on the parent when savechanges is called.
I can't write a test right now, but if needed I'll would write it this afternoon.
Is this the expected behaviour or a bug?
entity.OrderLine().arrayChanged.subscribe(function (args) {
        console.log(args);
        if (args.added && args.added.some(function (element) {
            console.log(element.entityAspect.entityState.name);
            return !(element.entityAspect.entityState.isUnchanged()
                || element.entityAspect.entityState.isDeleted());
        })) {
            console.log("modifico");
            entity.entityAspect.setModified();
        }
        if (args.removed && args.removed.some(function (element) {
             console.log(element.entityAspect.entityState.name);
            return !element.entityAspect.entityState.isAdded();
        })) {
            console.log("modifico");
            entity.entityAspect.setModified();
        }
    });

A: The parent is not changed automatically by the addition of a child because no data property of the parent changes. That is the technical reason.
Sometimes (often?) the model semantics say that the parent is changed by any addition/deletion/change-to a child. That is not always true which is why Breeze doesn't propagate the change automatically. But it is often true ... and I think it would be a good idea for Breeze to support this for you if you specify this as desired behavior in the metadata. You are not alone in wanting this.
I've added a User Voice suggestion for this idea; please vote for it if it (and add your comments) if it matters to you.
Meanwhile, in an entity initializer you can subscribe to changes in the parent collection and to the items of that collection and have them set the parent to the "Modified" state (parent.entityAspect.setModified()). This will have to do for now I'm afraid.

redpajama_set_name: RedPajamaStackExchange


Strike Force Heroes is an awesome shooting game online and you can enjoy it at KiZi Games! There are 3 modes in the game: Campaign, Challenge and Quick Match. Play the Campaign mode for a fully voiced, action-packed story, or create a custom match in the Quick Match mode. Try to complete all 15 challenging missions in the Campaign. Level up 4 unique classes and unlock over 65 weapons, multiple skills and kill-streaks. Use your arrow keys or W,A.S,D to move, jump and crouch. Move your mouse cursor to aim, click to shoot. Press Q or shift to switch your weapons.


programme to the maximum number of schools & colleges across the country.
Purpose: ADR has started CAP in 2018 to engage college students in political & electoral reforms process proactively. Eligibility: Anyone pursuing Graduate and Post Graduate regular courses with a passion to be a Change-Maker can be ADR Campus Ambassador. Training: The selected Campus Ambassadors are apprised about the issues ADR is working on & their roles and responsibilities as ADR campus representative. Activities: The Ambassadors are required to organize at least 6 major activities, like Panel Discussions, Quiz Contest, Film Festival, Street Play/Poster/Speech Competition etc. All the on Campus activities are approved, sponsored, assisted & supervised by the ADR Team. To apply for our Campus Ambassador Programme, keep checking our social media pages.


text:
Traffic signal still not up at Austin High School in Decatur. Here's why
Parents told WAAY 31 it's a major concern for them
Posted: Jan 16, 2020 6:04 PM
Posted By: Ashley Carter
Decatur City Schools said it will take up to a year and a half to build a traffic light to keep students safe.
The school district's project manager said the poles needed to build the light are out of stock.
In May, the district rolled out a plan to add a traffic light to the front entrance of Austin High School.
"It's hectic, very dangerous," Teresa Satchel, a parent, told WAAY 31.
Satchel said she's hesitant about letting her daughter in the 10th grade drive to school because of it.
"I'm constantly up here and I just see a lot of stuff," she said.
Official said the project isn't delayed, but that getting this traffic signal up is just a process and the mast arm traffic signal they are going to put up requires certain types of materials that they have to order from the Alabama Department of Transportation.
"It's crazy because we needed it when they built the school," Satchel said.
While Satchel wishes the light was here already, others don't believe it's needed at all
"If people know how to drive then i mean it's a stop sign, you know if cars are coming are not," PJ, who drives to the school frequently, said.
But, Satchel says when people are in a hurry it's easy to ignore the stop sign and take risks.
"The children, they're gonna take a chance because they're rushing sometimes because they're late and i've seen them just take a chance," she said.
The district said it will be until at least November before the new signal is up.
Decatur Utilities still working to get traffic signals working
Athens power outage impacts traffic signals
Traffic alert: Traffic signals out at Hughes Road, Madison Boulevard
Traffic signal coming to dangerous intersection in Limestone Co.
Capacity limited for Decatur-Austin football game
Juveniles charged after theft reported at new Austin High School in Decatur
Alabama Bicentennial celebrated at Decatur High School
High school football practice begins in Decatur


CASWELL DEVELOPMENTAL CENTER, DEPT. OF HEALTH & HUMAN SERVICES, Respondent.
Heard in the Court of Appeals 20 March 2018.
Appeal by respondent from final decision and award entered 23 June 2017 and 6 July 2017 by Administrative Law Judge Melissa Owens Lassiter in the Office of Administrative Hearings No. 16 OSP 12067.
Glenn, Mills, Fisher & Mahoney, P.A., by Daniel N. Mullins, for petitioner.
Attorney General Joshua H. Stein, by Assistant Attorney General Milind K. Dongre, for respondent.
Caswell Developmental Center, North Carolina Department of Health and Human Services ("Respondent") appeals from the final decision of the administrative law judge ("ALJ"), which reversed Respondent's decision to suspend Tankita Peterson ("Petitioner") for five days without pay. We affirm the decision of the ALJ.
Caswell Developmental Center ("Caswell") is a state-run facility operated by the North Carolina Department of Health and Human Services. Caswell provides care to residents who have disabilities, behavioral challenges, or medical conditions that require 24-hour care and supervision. Petitioner is a career state employee and has been employed at Caswell since October 2009. Petitioner was assigned to work the morning shift from 6:00 a.m. to 2:30 p.m. at the Magnolia Cottage, where five patients resided.
On 2 June 2016, Petitioner overslept to timely report for work. She awoke at approximately 6:20 a.m., and arrived at work at 7:00 a.m., an hour after her scheduled start time. On 6 June 2016, Petitioner received a documented counseling memo for unacceptable personal conduct on 2 June 2016 for her failing to report to work as scheduled and failing to notify her supervisor of her need to be late prior to the scheduled start of her shift, in violation of Caswell's Policy 4.9 Supervisor Notification of Absence. The memo further noted that violation of Policy 4.9 is an unexcused absence. Petitioner refused to sign the memo, because she "d[id] not agree . . . at all."
On 27 August 2016, Petitioner again overslept. She was awakened by a phone call from a colleague at approximately 6:30 a.m., and arrived for work at 7:00 a.m. Petitioner was issued a notice of pre-disciplinary conference on 5 September 2016, requesting she attend the pre-disciplinary conference the next day. The notice informed Petitioner of the possibility of a suspension without pay due to Petitioner's unacceptable personal conduct of reporting to work late and for failing to notify her supervisor on 27 August 2016, in violation of Policy 4.9 and Policy 5.1.46 Time and Attendance.
Petitioner was given the opportunity to respond to the proposed suspension without pay at the pre-disciplinary conference on 6 September 2016. In her written statement, Petitioner acknowledged she had overslept on 27 August 2016, and the alarm clock, which had failed to wake her up on that day, had previously failed before.
1) conduct for which no reasonable person should expect to receive prior warning, 2) conduct unbecoming a State employee that is detrimental for state service and 3) willful violation of known or written work rules [i.e., Caswell Developmental Center Administrative Policy Manual #5.1.46 (Time and Attendance) and Developmental Technician Manual #4.9 (Supervisor Notification of Absences)]. Specifically, [reporting] to work late and fail[ing] to notify a supervisor of [Petitioner's] need to be late from work, according to policy.
Petitioner's supervisor referenced the previous documented counseling for the same issue on 6 June 2016, and Petitioner's in-service training on the violated policies on 22 January 2016 and 6 June 2016.


You are visiting the placeholder page for Joseph Bailey. This page is here because someone used our placeholder utility to look for Joseph Bailey. We created this page automatically in hopes Joseph Bailey would find it. If you are not Joseph Bailey, but are an alumni of Arkadelphia High School, register on this site for free now.


text:
Paul Newman Blue eyes and politics
Photographer: Solange Podell
Article: Cyriaque Griffon
This quote could have been taken from a newspaper dated November 2016, referring to the run-up to the U.S. elections and iconic figures either supporting Hillary Clinton such as Meryl Streep, Beyonce, Cher and Madonna, or Donald Trump with celebs like Mike Tyson, Chuck Norris, Paul "Hulk" Hogan, Clint Eastwood, Jean-Claude Vandamme and Kirstie Alley.This quote is taken from the Time weekly magazine issue dating May 1968 though. And that was already true at a time when celebrity participation in the presidential primary and general elections of the United States reached an unprecedented level.
Pretty like today, the Hollywood participation was prominent among Democrats but also a key factor in the Republican races. Eugene McCarthy announced his candidacy for the Democratic Party for the White House. Facing him, Richard Nixon was campaigning on the Republican side. In the years 1967 – 1968, there was a boiling caldron of social issues and political unrestliken ever before. The students and the hippies would demonstrate on the streets and Luther King had just been assassinated. One of the Democrats' main issues was opposing the war raging in Vietnam. The most important Hollywood star who came out for the Democratic Senator McCarthy was Paul Newman. The then novice photographer Solange Podell just happened to beat the right place at the right time to take a series of unforgettable snapshots of Newman when the actor was committed to supporting the Democrat candidate. The scene took place at the St-Regis, the most opulent and grand hotel in New York. This legendary hotel had, among his most famous residents, Salvador Dali. The artist would spend his winters there. This was the place where Marilyn Monroe stayed had when filming the famous subway grate scene in The seven-year sitch. St-Regis Hotel, New York, 1968
I was told that Paul Newman was about to come to the St-Regis Hotel and attend a cocktail reception held in support of the Democratic senator McGovern in the primary elections, Solange recalls. I was sent to the St-Regis by the famous American photographer Santi Visalli (who worked for Photoreporters agency).When I arrived, there he was, standing in front of me. He was as smart and handsome as I had expected, wearing an elegant dark suit with a bowtie, holding a glass in one hand. A screen legend with one of the most magnetic piercing steel blue eyes in movie history. On that day, that was for me a wonderful opportunity to take a series of photos.
I remember that dark-haired female reporter in a blue dress with a notepad in one hand. She seemed to be clumsy when asking questions and Newman did not bother really. As he was well educated he pretended to be interested in her questions. Yet, he started looking around, obviously feeling like doing one thing, getting away from that journalist. And when he caught my eyes, I caught his eyes too and started snapping away at him. His piercing look made me think of a « call for help.On that day, I had a little bit the sentiment that I had helped him in some way, enabling him to get away from the reporter.
McGovern lost in the primaries and Newman went on supporting the elected Democrat McCarthy. The latter lost. That earned Newman a charter list on the new elected Republican President Richard Nixon's Enemies List, right at number 19!
Tags 1967 Beyonce Blue eyes Cher Cyriaque Griffon Donald Trump Hillary Clinton Hollywood Madonna NEW YORK Paul Newman politics Solange Podell
Mahmoud Al Rifai
UK's leading Etiquette expert offers homeowners top tips to avoid upsetting the neighbours
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Dukla (do 1954 m. Dukla + gminy: Nadole i Tylawa) – gmina miejsko-wiejska w województwie podkarpackim, w powiecie krośnieńskim. W latach 1975–1998 gmina położona była w województwie krośnieńskim. Siedzibą gminy jest Dukla.

Według danych z 31 grudnia 2020 gminę zamieszkiwało 14 388 osób.

1 stycznia 2010 z gminy Dukla wydzielono gminę Jaśliska, obejmującą miejscowości Czeremcha, Daliowa, Jaśliska, Lipowiec, Posada Jaśliska, Szklary, Wola Niżna i Wola Wyżna.

Struktura powierzchni
Według danych z roku 2002 gmina Dukla ma obszar 332,5 km², w tym:
 użytki rolne: 41%
 użytki leśne: 52%

Gmina stanowi 36,05% powierzchni powiatu.

Demografia
Dane z 31.12.2017 roku.

 Piramida wieku mieszkańców gminy Dukla w 2019 roku

Sołectwa
Barwinek, Cergowa, Chyrowa, Głojsce, Iwla, Jasionka, Lipowica, Łęki Dukielskie, Mszana, Myszkowskie, Nadole, Nowa Wieś, Olchowiec, Równe, Teodorówka, Trzciana, Tylawa, Wietrzno, Zawadka Rymanowska, Zboiska, Zyndranowa

 Miejscowości niesołeckie
Granica, Kamionka, Ropianka, Smereczne, Wilsznia

Sąsiednie gminy
Chorkówka, Iwonicz-Zdrój, Jaśliska, Krempna, Miejsce Piastowe, Nowy Żmigród, Rymanów.

Gmina na południu sąsiaduje ze Słowacją.

Przypisy