text:
Labour will 'reconnect' Britain with Europe if it wins power
Shadow foreign secretary David Lammy promises a raft of fresh co-operation with European countries but says it will not roll back Brexit
Britain's shadow foreign secretary David Lammy at Chatham House, London. He said if Labour wins power it will rebuild bilateral relations with countries such as Ireland, France and Germany. Photograph: Neil Hall/EPA
Mark Paul in London
Tue Jan 24 2023 - 18:46
A Labour government would "reconnect" Britain with its international partners and be "a good neighbour ... [and] a leader in Europe once again," according to a landmark foreign policy speech by David Lammy, the shadow foreign secretary.
Mr Lammy told an audience at the Chatham House think tank in London on Tuesday that if Labour wins power it will rebuild bilateral relations with countries such as Ireland, France and Germany. He also promised to forge a new security pact with the European Union, with regular summits to discuss shared priorities such as imposing sanctions and maintaining energy security.
"Reconnecting Britain to Europe, while remaining outside the EU, will be a top priority," said Mr Lammy. He also reiterated Labour's three promises on Brexit – that it will not rejoin the Single Market, the Customs Union or the EU itself.
Mr Lammy suggested that in the years following Brexit, Britain has "lost" its place in the international order. "Britain feels lost and disconnected in a world that is more divided than at any other time since the fall of the Berlin Wall ... We have left the EU but not yet found a new, settled and confident place in Europe."
Germany's CDU faces headache over ex-spy chief's refusal to leave party amid racism claims
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Volunteering key to British creed of keeping calm and carrying on
He deliberately echoed the language of Brexiteers by declaring a pillar of a Labour government's approach to foreign policy would be to "take back control".
"The Brexiters were right about that, but fundamentally wrong to think it means going alone."
He identified three big trends shaping the foreign policy landscape. A new age of geopolitical competition with the world economy splitting into blocs as rivalry between US and China "shapes our century". The second is the "weaponised interdependence" of global economies and supply chains, with the risk that new technologies such as artificial intelligence could be "tools of authoritarian power". He also echoed US worries about "blurring the distinction between domestic and foreign policy".
In reconnecting Britain with its traditional partners, he promised Labour would put "pragmatism before ideology" and fix "institutional dysfunction" at the heart of the government department that runs UK foreign policy, the Foreign, Commonwealth and Development Office (FCDO).
The FCDO would be overhauled to focus more on creating policies to help Britain reach climate goals, grow its economy, improve security and retune international development policy and diplomacy.
Mr Lammy promised that under Labour Britain would "stand with Ukraine for the long haul". He also lamented that Britain had been "locked out" of the EU's diplomatic process, and promised to bring his nation's "heft" to fresh co-operation with the EU on security.
FCDO, he said, would link up with the Home Office to bring together the intelligence and security communities, creating a new "state threats cell" to give an early warning system for threats.
He said Labour would use a planned 2025 review of its Brexit withdrawal deal to "reduce barriers to trade". He said he also hoped to improve relations with the US, highlighting how they flourished under Tony Blair's New Labour project.
He said that whenever he is in the US he detects that "the chaos of the UK is not seen as a joke, it is seen as a problem".
"It will fall to us to rebuild the foundation of our influence in the world."
Mark Paul
Mark Paul is London Correspondent for The Irish Times
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text:
Twice Jailed, Thrice Shy: Kung Raiya Ends Activism Over Safety Fears
| Wed Jul 14, 2021 5:30 pm
Kung Raiya stands in front of an overturned motorbike on a driveway, rubbing a scab on his elbow. (Supplied)
Kung Raiya says these days he just sells honey online from his shop, but even doing deliveries for the business has been fraught with danger.
As a 25-year-old university student in 2015, Raiya was arrested over a Facebook post calling for a "color revolution" in the country. He spent 18 months in prison for incitement before his release in 2017.
He was still defiant at the time, telling The Cambodia Daily that he would continue to advocate for his country. "First, I would like to thank the government who put me in jail," he said in 2017. "Because this experience in prison has made me strong."
In 2019, Raiya was again arrested in Phnom Penh on the third anniversary of the murder of political analyst Kem Ley for printing T-shirts with Ley's words and image.
"If you do nothing, you will certainly suffer; it is just not your turn yet," the T-shirts said, quoting Ley.
At the time of his second arrest, he was married and had a small child.
Raiya was released on bail later that year, and went to Thailand for medical treatment before seeking asylum abroad.
But Raiya, speaking to VOD earlier this month, said he had returned to Cambodia in November so that he could be close to his family. Now in his 30s, Raiya said he had hoped he would be able to develop his honey business.
But in December, a little over a month after his return, he saw a stranger lurking around his house. When he went out for a delivery on his motorbike, he saw the same man drive up to him and kick him over.
Raiya said his helmet spared him from serious injury, but he had gashes on his elbows and knees from being scraped along the road.
Since then, he had barely left his house, Raiya said. He also was done speaking out about issues plaguing society, he said.
"For the matter of social expression, it is related to safety, because now my safety seems to be very fragile, making me worry and fear for my safety if I were to continue to criticize or publicly talk about social issues," he said.
He kept an eye on what was happening, but political activity was behind him, he said.
The choice over whether to continue to speak out in Cambodia has also racked members of the main opposition CNRP, which was dissolved and outlawed by the Supreme Court in 2017.
A former party youth activist in Phnom Penh, who declined to be named for fear of repercussions, said he had also fled to Thailand for about a month. Since returning, he had received repeated threats, mostly on social media, the activist said.
Now, he had stopped posting online about political issues and severed his links with the CNRP, and the threats gradually decreased, he said. He had feared for his personal safety and had a business to run, he said.
"Now we live a normal life. We cannot do anything, just live to keep safe and for family life. We just adapt to that," the man said.
Sin Chanpeou Rozeth, a former commune councilor in Battambang, said she also faced pressures and a tough decision about continuing her activism.
She — or her family members — could be attacked at any time, anywhere, like other former CNRP activists had been, she said.
But she still wanted to speak out about the country's issues, Chanpeou Rozeth said.
"Sometimes we have to take risks too. We don't know when it will be our turn, when we will be accused, if we continue to criticize," she said. "But even if we do not show care for our nation, we still know and see the deeds, and if we do not dare to speak, the significance of our lives for this national society will be unknown."
CNRP vice president Mu Sochua has said that 31 former opposition activists have been attacked in Cambodia since 2017.
However, Chin Malin, spokesperson for the Justice Ministry and the Cambodian Human Rights Commission, dismissed claims that freedom of expression in Cambodia was restricted, especially for former CNRP political activists.
All citizens, including supporters of political parties, have the right to express themselves freely, but they must do so in accordance with the law, Malin said.
"A small number of these activists have had legal problems in the past, not because of a lack of freedom of expression, but because of violations of the law, such as defamatory expressions, infringing on the dignity of others' privacy, inciting social unrest and such," he said. "We see the vast majority of people using social media, they express themselves freely without any problems. Why does only this small group have problems?"
cnrp, kung raiya, Mu Sochua, opposition, political rehabilitation

redpajama_set_name: RedPajamaCommonCrawl


text:
Wimbledon final: Murray's return takes on Raonic's serve
The sixth-seeded Raonic heads into the first Grand Slam title match of his career and the first for a man representing Canada having won 116 of his 121 service games (96 percent) across six matches.
London 10 July, 2016 13:01 IST
In his five-set victory over Roger Federer in the semi-finals, Raonic saved 8 of 9 break points. He went as high as 144 mph more than once with his serve and his average first serve of 129 mph was faster than Federer's best offering of 126 mph. - Getty
Milos Raonic is as good a server as there is in tennis nowadays. Andy Murray is one of the top returners.
"Obviously," said Murray, the 2013 Wimbledon champion, "Milos has got a fantastic serve."
Raonic, who added John McEnroe to his coaching staff ahead of the grass-court portion of this season, has hit 154 aces, averaging 25 per match. He's faced only 27 break points, saving 22.
>READ: Raonic confident in his armoury ahead of Murray final clash
In his five-set victory over Roger Federer in the semi-finals, Raonic saved 8 of 9 break points.
Not only did the 6-foot-5 Raonic repeatedly top 140 mph in that match, he went as high as 144 mph more than once, and his average first serve of 129 mph was faster than Federer's best offering of 126 mph.
Raonic's serve is speedy and scary, to be sure British Davis Cup captain Leon Smith called it "ginormous" but it is also much more than that.
One reason it's so effective is because of his ability to alter velocity and placement.
Against Federer, he would boom one right at the body at upward of 135 mph emanating a thud that reverberated around Centre Court then hit an ace out wide at 115 mph that sent up a spray of chalk when it hit a line.
"You don't get in a rhythm," said Sam Querrey, the American who lost to Raonic in the quarterfinals after beating No. 1 Novak Djokovic in the third round. "You go games on his serve where you might get one return in play."
Don't count on that happening too often against Murray.
Take out players who didn't make it past the second round this fortnight, and the second-seeded Murray ranks No. 1 in-percentage of returns put in play, 77; percentage of second-serve points won, 64; percentage of return games won, 36.
Murray a two-time major champion, most famously becoming the first British man to win Wimbledon in 77 years has won his past five matchups against Raonic. Just three weeks ago, Murray won their meeting in the final of the Queen's Club grass-court tournament. Murray dropped the first set, then trailed 3-0 in the second, before beginning the turnaround with a return winner.
>READ: Murray, Raonic look to super coaches for Wimbledon glory
"It helps to have played a match against him on the grass," Murray said. "You know, see some of the things he's doing on this surface a little bit differently."
For Murray, this will be the 11th Grand Slam final of his career and third of this year but first against someone other than Djokovic or Federer.
Raonic was asked what sort of a boost his debut in a major final might be for Canadian tennis.
"It's great to sort of be at the center and front of that come Sunday. I'm glad that I've sort of been leading this charge, the first one to break through and really put these things together," he said. "But I'm by no means done."
Both times Murray earned a major trophy, Ivan Lendl was his coach. And after a hiatus, they have reunited.
"I don't think it's a coincidence. I obviously had the best years of my career with him," Murray said.
"I obviously wanted to work with Ivan again to try to help me win these events," he added. "That's the goal."
One of eight-time major champion Lendl's rivals during his playing days was McEnroe, who won three of his seven Grand Slam titles at Wimbledon. Lendl won 21 of their 36 head-to-head matchups, although McEnroe won the only time they played at the All England Club, in the 1983 semi-finals.
Lendl is expected to be seated in Murray's guest box at Centre Court for the final. McEnroe? Instead of supporting Raonic at courtside, he'll be in the TV commentary booth, calling the match for ESPN.


text:
Dětské dopravní hřiště (německy Verkehrsgarten, "dopravní zahrada") je plocha určená k dopravní výchově dětí. Je na ní umístěna zmenšená modelová síť ulic, silnic a chodníků s různými dopravními značkami a dopravními zařízeními, například světelnými semafory. Používají se zejména ke školou organizované dopravní výchově, ale některá dopravní hřiště jsou přístupná veřejnosti i individuálně. Na některých dopravních hřištích provozovatel zapůjčuje dětem jízdní kola nebo umožňuje použití jejich vlastních jízdních kol či koloběžek, někde probíhá výuka bez vozidel tak, že děti představující vozidla po vozovce pouze procházejí či probíhají. V západní Evropě je běžnější používat šlapací nebo elektrická autíčka.

První dětská dopravní hřiště vznikala již ve 30. letech 20. století, nedlouho po zavedení dopravního značení a silniční dopravní signalizace.

Dětská dopravní hřiště v Česku a na Slovensku
Dopravní hřiště byla v Československu budována od počátku 80. let 20. století.

V České republice byl systém dopravní výchovy s jejich využitím nadále průběžně rozvíjen. Provozovateli dětských dopravních hřišť jsou základní a mateřské školy, autoškoly, domy dětí a mládeže a střediska volného času, AMK (Automotoklub), obce, Česká i městské policie i další subjekty včetně soukromých. Ve většině českých okresů je jedno nebo více dopravních hřišť, v Praze jich je devět.

Standardy dopravního vzdělávání počítají s tím, že základy pravidel silničního provozu by si dítě mělo osvojit nejpozději do 10 let věku, odkdy smí samostatně jezdit po pozemních komunikacích na jízdním kole. V rámci programu připraveného Ministerstvem dopravy ČR probíhá zpravidla ve čtvrtých třídách základních škol (případně ve třetí nebo páté třídě) systematický výcvik jízdy na kole, doporučují se dvě návštěvy třídy na dopravním hřišti v průběhu školního roku o celkovém rozsahu praktické výuky 5 hodin (například 3 hodiny na podzim a 2 hodiny na jaře). Po úspěšném završení teoretické i praktické výuky dítě dostává takzvaný "průkaz cyklisty", který však je jen symbolický a nemá žádné právní dopady.

Na Slovensku počet dopravních hřišť klesl z 54 v roce 1989 na 34 v roce 2005. V roce 2005 byla vládními orgány přijata nová koncepce udělování licencí k dopravní výchově a v roce 2006 byly ministerstvem školství vyhlášeny podmínky pro získávání dotací pro provozovatele dopravních hřišť a poskytovatele dětské dopravní výchovy. Nové osnovy dopravní výchovy od roku 2005 předpokládají 2 hodiny praktické dopravní výchovy ročně v 1. až 3. třídě a 4 hodiny na dopravním hřišti během 4. třídy.

Literatura
 BESIP: Výcvik na dětských dopravních hřištích, Edice dopravní výchovy, č. 14/1997
 BESIP: Metodický list k činnosti dětských dopravních hřišť

Externí odkazy

 Seznam dopravních hřišť v Česku ve formátu XLS

 László Szigeti, ministr školství Slovenské republiky: Vyhlásenie podmienok k poskytovaniu dotácií na financovanie výchovy a vzdelávania v oblasti zvyšovania bezpečnosti v premávke na pozemných komunikáciách a v oblasti praktického výcviku žiakov základných škôl na detských dopravných ihriskách. (5. dubna 2006)
 The Daily Herald Archive: Children's traffic playground, 1938 Fotografie dětského dopravní hřiště v Londýně (Tottenham) z roku 1938

Silniční doprava
Dopravní stavby
Dopravní výchova
Dětské hřiště

redpajama_set_name: RedPajamaWikipedia


An unprecedented event in the winter of 2007 left the scientific community in shock. In the state of New York, thousands of bats were found dead in four caves, and its believed that numerous others had perished outside their shelters. This hypothesis coincided with an increase by a factor of ten in the number of dead specimens from the genus Myotis.
After initial uncertainty, today it is known that the cause of that massive die-off was the fungus Pseudogymnoascus destructans, or Pd. Originally from Eurasia, it likely arrived to North America by human action and over the past decade this fungus has spread across the United States and seven provinces of Canada eliminating more than seven million bats. What's worse, it continues to advance and appears unstoppable.
Pd attacks the tissues while bats hibernate, causing discomfort in the patagium (the skin membrane that forms the surface of the wing) and snout, thus generating the characteristic white spots that gave rise to the name of the disease In English: white-nose syndrome (also known as W.N.S.). The disease causes bats to wake from their hibernation state, and thus spending their energy reserves which leads them to eventually die in flight or inside their shelters.
In 2016, we began a project that will allow us to know in stages whether the fungus is present in Chilean Patagonia and what to do to fight it or control its arrival. Currently, the research is being carried out in parts of Karukinka Park, on the Chilean side of Tierra del Fuego island, where we have captured individuals of Myotis chiloensis and Histiotus magellanicus, both non-migratory species and, therefore, they are hibernating there. The first results confirm that the bat populations in this part of Patagonia are free of the feared W.N.S., but at the same time we also conclude that they are susceptible to becoming contaminated.
That is why in 2017 we began monitoring environmental conditions in ten abandoned caves and mines throughout the rest of Chile to determine whether they are at risk of contamination by the fungus. The results of the project are expected to provide the basis for an action plan to prevent the arrival of W.N.S. to Chile.


Kim Getty | AdForum Talent: The creative industry network.
As President of Deutsch's Los Angeles office, Kim leads a world-class team of entrepreneurial thinkers who roll up their sleeves to help businesses grow. Since joining Deutsch in 2003, Kim has been instrumental in building the agency into one of the most innovative creative shops on the west coast. During her tenure at Deutsch, she has driven the development of new practice areas for the agency, including experiential marketing, music, PR and DLAtino.
Committed to nurturing young talent, Kim serves as an adjunct professor at USC's Annenberg School and also sits on the board of The Grady College of Journalism and Mass Communication at the University of Georgia. Kim has been recognized as one of the most powerful women in advertising by Business Insider, a top LA executive by the Los Angeles Business Journal, and earned the American Advertising Federation's Mosaic Award for Industry Career Achievement. She is also a regular contributor to Fortune and Entrepreneur.
Same breakfast, same muffin, same smile.
•	DEUTSCH LA: For upgrading its ad agency into a product developer too. If your kid is now convinced that he can start the car using the Force, or if a chorus of dog barks replaces the tune of the "Imperial March" in your head, you have Deutsch LA to thank. After many years of creative dormancy, the storied agency has reached a new creative stride in the past few years, owed largely to these Super Bowl spots for Volkswagen. Deutsch LA has also invested heavily in product development with its Inventionist unit, going beyond advertising to produce mobile apps for brands like Pop Secret.
Started the Deutsch Moms Group, bringing in a licensed therapist and parenting consultant monthly to field questions and support the agency's community of moms.


text:
#include "./DirectX9Private.h"

#include "alkes/directx9/DirectXImageBufferFactory.h"

namespace alkes {

DirectXImageBufferFactory* DirectXImageBufferFactory::create(IDirect3DDevice* device)
{
    return device ? new DirectXImageBufferFactory(device) : NULL;
}

void DirectXImageBufferFactory::destroy()
{
    delete this;
}

DirectXImageBufferFactory::DirectXImageBufferFactory(IDirect3DDevice* device)
: device_(device)
{
}

DirectXImageBufferFactory::~DirectXImageBufferFactory()
{
}

ImageBuffer* DirectXImageBufferFactory::createImageBuffer(uint16_t width, uint16_t height, PixelFormat format, bool /*write_only*/)
{
    return DirectXImageBuffer::create(device_, width, height, format);
}

}

redpajama_set_name: RedPajamaGithub


suthepphoto.com -Renovations Remodeling Renovation (also called remodeling) is the process of improving a broken, damaged, or outdated structure. Renovations are typically either commercial or residential.
Insideout renovations. InsideOut Renovations is a leading provider in home remodeling and renovations in Lincoln, Nebraska.


text:
\section{INTRODUCTION}

Expanding H{\sc ii} regions or supernova explosions can strongly influence their surrounding interstellar medium (ISM) and regulate star formation. The shocks induced
in H{\sc ii} regions or supernova remnants may gather surrounding molecular gas to form dense shells, which may collapse to form stars later \citep{el77,whit94}.
This so-called ``collect and collapse" process can self-propagate and lead to sequential star formation \citep{el77,whit94}. The ``collect and collapse" model was firstly developed to explain the age sequence of spatially
distinct OB subgroups in nearby OB associations such as Orion OB1 \citep{el77}. More and more evidences in recent observations indicate that new generation of stars can form in shells or pillar structures surrounding H{\sc ii} regions (see \citealt{liu12a,dale15,liu15,liu16a} and the references therein). \cite{thom12} estimated that the fraction of massive
stars in the Milky Way formed by triggering process could be between 14 and 30 $\%$ through statistical studies of young stellar objects (YSOs) projected against the rims of Spitzer infrared bubbles.

However, recent numerical simulations suggest that stellar feedback from massive stars always results
in a lower star formation efficiency and most signs such as the ages and geometrical distribution of stars relative to the feedback
source or feedback-driven structure (e.g. shells, pillar structures), may not be substantially helpful in distinguishing triggered star formation from spontaneous star formation \citep{dale12,dale15}.
Studying the conditions (e.g., temperature, density, velocity, chemistry) of dense cores near H{\sc ii} regions may be helpful to distinguish triggered star formation from spontaneous star formation.
The dense cores should be externally heated and compressed by H{\sc ii} regions if their star formation would be triggered.

The \textit{Planck} satellite survey provides a catalog containing 13,188 Planck Galactic cold clumps \citep[PGCCs;][]{planck15}.
The clumps have dust temperatures lower than 14 K, indicating that PGCCs correspond to the coldest portion of the ISM.
A survey in the $J$ = 1--0 lines of $^{12}$CO, $^{13}$CO, and C$^{18}$O toward 674 PGCCs, has been carried out using the 13.7 m telescope of Purple Mountain Observatory (PMO) \citep{wu12,liu13,zhang16}.
Nearly 98 $\%$ of the clumps have the excitation temperatures ($T_{\textrm{ex}}$) of CO 1--0\ lower than 16 K.
Clumps with excitation temperatures above 16 K are located in star-forming regions, suggesting that the high $T_{\textrm{ex}}$\ is related to star-forming activities \citep{wu12}.
A large fraction of PGCCs have lower temperatures than the typical temperature of Infrared dark clouds (IRDCs) \citep[15 K;][]{pillai06}, which are known to be the earliest phase of star formation \citep{carey98,simon06}.
It suggests that PGCCs may represent an earlier evolutionary stage than IRDCs.
To investigate the initial conditions of star formation, and especially to study the environmental effect on dense core formation, a legacy survey of PGCCs using the Submillimeter Common User Bolometer Array-2 (SCUBA-2) on board of the James Clerk Maxwell Telescope (JCMT) at East Asia Observatory, ``SCUBA-2 Continuum Observations of Pre-protostellar Evolution (SCOPE\footnote{https://topscope.asiaa.sinica.edu.tw/tiki/tiki-index.php})" is in progress (liu et al. 2017, in preparation).

PGCC G108.84--00.81\ is observed as part of SCOPE.
It has an excitation temperature of $\sim$15 K and H$_2$\ column density of 2.0 $\times 10^{22}$ cm s$^{-1}$ \citep{wu12}.
Hereafter we call the region covered by PMO observations (500\arcsec $\times$ 500\arcsec) as PGCC G108.84--00.81\ and the central part of PGCC G108.84--00.81\ covered by SCUBA-2 as G108.
A supernova Remnant (SNR) G109.1--1.0 and an H{\sc ii} region, Sh2-152, are located near PGCC G108.84--00.81.
Therefore, PGCC G108.84--00.81\ is an ideal target to investigate the environmental effect on the initial conditions of star formation.

In this study, we investigate the interaction between PGCC G108.84--00.81\ and its surrounding environments with CO line observations.
The chemical and physical properties of G108 are also studied in detail through a series of observations in both continuum and molecular lines.
In Section 2, our observations toward PGCC G108.84--00.81\ and G108 are summarized.
Results and analysis are presented in Section 3 and Section 4, respectively.
We discuss the environmental influence on the star formation in PGCC G108.84--00.81\ in Section 5.
Finally, a summary of the study is given in Section 6.

\section{THE DATA}

A series of observations toward PGCC G108.84--00.81\ have been conducted with ground-based radio telescopes.
The reduction process of molecular line data was done using the GILDAS/CLASS\footnote{see http://www.iram.fr/IRAMFR/GILDAS/doc/html/class-html/class.html.} package.
A summary of the molecular line observations is in Table 1.

\subsection{PMO Observations}
The CO 1--0, $^{13}$CO 1--0, and C$^{18}$O 1--0\ line mapping observations of PGCC G108.84--00.81\ were carried out using the 13.7 m radio telescope of the PMO at De Ling Ha in 2011 May.
The On-The-Fly (OTF) observing mode was applied.
More details of the OTF observations with the PMO 13.7 m telescope toward Planck cold clumps can be found in \citet{liu12}.
The beam Full Width at Half Maximum (FWHM) is $\sim$52$\arcsec$ at 115 GHz and the beam efficiency is $\sim$0.45.
Newly installed nine-beam array receiver in the single-sideband mode was used.
The Fast Fourier Transform Spectrometer (FFTS), which has 16,384 channels in a total bandwidth of 1 GHz, were used.
The velocity resolution of the CO 1--0\ line is 0.16 km s$^{-1}$ and that of both $^{13}$CO 1--0\ and C$^{18}$O 1--0\ is 0.17 km s$^{-1}$.
CO 1--0\ was observed at the upper sideband and $^{13}$CO 1--0\ and C$^{18}$O 1--0\ were observed simultaneously at the lower sideband.
The map size for further analysis is about 480\arcsec$\times$480\arcsec.

\subsection{CSO Observations}

Molecular line observations of PGCC G108.84--00.81\ were carried out with the 10 m telescope of the Caltech Submillimeter Observatory (CSO) in 2014 January (see Meng et al. in preparation).
We mapped the CO 2--1, $^{13}$CO 2--1, and C$^{18}$O 2--1\ lines toward G108.
The Sidecab receiver and the FFTS2 spectrometer were used.
The velocity resolution is about 0.35 km s$^{-1}$.
The beam FWHM is 32.5$\arcsec$ and the beam efficiency is 0.76 at 230 GHz.
A map area of 120\arcsec$\times$120\arcsec\ centered at G108 is selected for further analysis because of apparent higher noise levels at map edges.

\subsection{NRO Observations}
The northern part and the southern part of G108 were observed separately with the 45 m radio telescope of the Nobeyama Radio Observatory (NRO) in 2015 December.
We observed N$_2$H$^+$ 1--0\ with the TZ1 receiver.
The velocity resolution is about 0.2 km s$^{-1}$.
The beam FWHM at 93 GHz is 20.4$\arcsec$ and the beam efficiency is 0.54.
Each mapped area toward the northern and southern part of G108 is 50\arcsec$\times$50\arcsec.

\subsection{IRAM Observations}
We also observed the HCO$^+$ 1--0\ and HCN 1--0\ lines toward the northern part of G108 with the 30 m radio telescope of the Institut de Radioastronomie Millim\'{e}trique (IRAM) in 2014 May.
The velocity resolution is 0.33 km s$^{-1}$.
The beam FWHM and beam efficiency are $\sim$29 $\arcsec$ and 0.81, respectively.
The map size is 80 \arcsec$\times$80 \arcsec.

\subsection{Effelsberg Observations}
Observations of the northern part of G108 in the NH$_{3}$ (1,1)\ line was carried out with the 100 m radio telescope of Effelsberg in 2015 April.
The NH$_{3}$ (1,1)\ line was observed with 1.3 cm double beam secondary focus receiver.
The beam FWHM and beam efficiency are $\sim$38 $\arcsec$ and 0.79, respectively.
The velocity resolution is 0.15 km s$^{-1}$.
An area of 80 \arcsec$\times$80 \arcsec\ was mapped.

\subsection{KVN Observations}
Single-point observations of the HCN 1--0\ line were carried out toward the peak positions of the 850 \micron\ dust continuum map in 2016 June with the Korean VLBI Network (KVN) 21 m telescopes \citep{kim11}.
Observations were conducted at the three stations of KVN (Yeonsei, Ulsan, and Tamna).
We used the digital spectrometer with 32 MHz in bandwidth divided into 4096 channels, providing velocity resolution of $\sim$0.2 km s$^{-1}$ at 88 GHz.
The averaged beam FWHM and beam efficiency at the three stations are $\sim$32$\arcsec$ and $\sim$0.39 at 88 GHz, respectively.

\subsection{JCMT Observations}
The 850 \micron\ continuum emission map was obtained with JCMT/SCUBA-2 in 2015 May in the "CV Daisy" mapping mode, which is optimised for point sources.
The CV Daisy is designed for small compact sources providing a deep 3$\arcmin$ region in the centre of the map but coverage out to beyond 12$\arcmin$ \citep{bint14}.
All the SCUBA-2 850 \micron\ continuum data were reduced using an iterative map-making technique \citep{chap13}.
Specifically the data were all run with the reduction tailored for compact sources, filtering out scales larger than 200$\arcsec$ on a 4$\arcsec$ pixel scale.
The beam FWHM of SCUBA-2 at 850 \micron\ is $\sim$13 $\arcsec$.
The field of view of SCUBA-2 is about 8 \arcmin\ at 850 \micron.
However, an area of about 5\arcmin$\times$5\arcmin\ entered at PGCC G108.84--00.81\ is used for further analysis.

Molecular line observations in HCO$^+$ 4--3\ toward the northern part of G108 were also carried out using the JCMT Heterodyne Array Receiver Program (HARP) system in 2015 September.
HARP is a Single Sideband array receiver composed of 16 SIS mixers.
The beam FWHM at 350 GHz is $\sim$14 $\arcsec$ and the beam efficiency is 0.64.
The mapping area is about 50 \arcsec$\times$50 \arcsec.
We used the "ORAC-DR" pipeline in STARLINK for imaging data reduction.

\subsection{Infrared Data}

We also included images from \textit{Wide-field Infrared Survey Explorer} (WISE) \citep{wright10}.
We gathered available photometric data of Young Stellar Object (YSO) candidates in G108 from several catalogs.
The data at 3.4, 4.6, 12, and 22 \micron\ are from the ALLWISE catalog including 2MASS data.
The data at 9 and 18 \micron\ are from the AKARI/IRC Point Source Catalogue \citep[AKARIPSC;][]{ishihara10}.

\section{RESULTS}

\subsection{Filament structure in the CO 1--0\ and $^{13}$CO 1--0\ maps}

PGCC G108.84--00.81\ is surrounded by dynamically active regions such as a supernova remnant, SNR G109.1--1.0, and an H{\sc ii} region, Sh2-152.
According to Planck Early Cold Clump catalog note\footnote{http://irsa.ipac.caltech.edu/Missions/planck.html}, there is one IRAS point source, IRAS 22565+5839, associated with PGCC G108.84--00.81\ within 5 arcmin from the center of PGCC G108.84--00.81.
One large filament structure is shown in the integrated intensity map of CO 1--0\ (Figure 1).

This filament structure is largely divided into three parts: the northeast region associated with a star \citep{yung14}, IRAS 22576+5843, the southern region directly linked to Sh2-152, and the central part defined as G108, containing IRAS 22565+5839.
As shown in the $^{13}$CO 1--0\ map in Figure 2, G108 is composed of two components.
One is located at northeast (NE) from the central position and the other is located at southwest (SW).
We use ``G108--N'' to indicate the NE component and ``G108--S'' for the SW component.

The systemic velocity of --49.6 km s$^{-1}$ has been measured by Gaussian fitting the C$^{18}$O 1--0\ spectra toward G108.
The nearby H{\sc ii} region, Sh2-152, has a similar systemic velocity to G108.
We adopt the distance to PGCC G108.84--00.81\ as 3.21 $\pm$ 0.21 kpc from the distance estimation of Sh2-152 by \citet{ramirez11} based on near-infrared extinction.
According to the moment 1 maps presented in Figure 2, a small velocity gradient is present at the SW part of PGCC G108.84--00.81.

\subsection{Two clumps within G108}

Figure 3 presents the integrated intensity maps of CO 2--1\ and $^{13}$CO 2--1\ overlaid onto their Moment 1 maps obtained at the CSO.
G108--N and G108--S seem separated in the CO 2--1\ map.
The integrated intensity map of $^{13}$CO 2--1\ presents more fragmented structures than that of CO 2--1.
The component with a blue-shifted velocity with regard to the systemic velocity ($\sim$ --50.5 km s$^{-1}$), is shown in the west of G108--S.
The red-shifted velocity components are located along the eastern edge of filament in the $^{13}$CO 2--1\ map.

The spectra of CO isotopologues obtained with the CSO telescope toward G108--N and G108--S are shown in Figure 4.
The central velocities of three lines are coincident with each other.
Figure 5 shows the integrated intensity ratios, CO 2--1$/$CO 1--0\ and $^{13}$CO 2--1$/$$^{13}$CO 1--0.
The enhancement of CO 2--1$/$CO 1--0\ ratios ($> 1$) are known toward molecular clouds associated with SNRs \citep{seta98}.
However, in G108, the $^{13}$CO 2--1$/$$^{13}$CO 1--0\ ratio is the most enhanced at the southern edge of G108--S, which is close to the H{\sc ii} region.

In Figure 6, the 850 \micron\ dust continuum emission map is overlaid onto the WISE 12 \micron\ image.
Dust continuum emission toward G108 is also largely divided into two parts (G108--N and G108--S), as molecular line emission.
Distribution of dust continuum emission of G108--N shows a cometary structure.
The head is located at the NE from the center with a tail structure extended to SW.
Highly fragmented structure appears in G108--S.
At least four components exist in G108--S.
G108--S1 to S4 are assigned along with Right Ascension.
As shown in the integrated intensity maps of CO 2--1, $^{13}$CO 2--1, and C$^{18}$O 2--1\ overlaid onto the 850 \micron\ dust continuum emission map (Figure 7), the intensity peaks of all three lines are off from that of the dust continuum.

\subsection{A starless clump, G108--N}
To investigate the molecular environments of the starless clump, G108--N, single-dish observations were conducted.
The integrated intensity maps of HCO$^+$ 1--0\ and HCN 1--0\ obtained with the IRAM 30 m telescope are shown in Figure 8.
The HCO$^+$ 1--0\ and HCN 1--0\ show a similar distribution to each other and also to the distribution of 850 \micron\ continuum emission.
The peak positions of HCO$^+$ 1--0\ and HCN 1--0\ are slightly shifted from that of the 850 \micron\ continuum emission peak.
The emission of the two lines distributes along the cometary structure in the NE-SW direction.
The head at the NE with a tail extended to SW is shown in HCO$^+$ 1--0\ and HCN 1--0\ maps while HCO$^+$ 4--3\ obtained with the JCMT/HARP shows a compact distribution near the head part (Figure 8c).
This cometary structure is also shown in the integrated intensity map of NH$_{3}$ (1,1)\ obtained with the Effelsberg 100 m telescope (Figure 9).

The line profiles of all observed molecular lines toward the 850 \micron\ dust continuum peak of G108--N are presented in Figure 10.
The centroid velocities of all lines are consistent.

\section{ANALYSIS}

\subsection{IR source in association with G108}
G108--N has no associated infrared (IR) source.
On the other hand, two IR sources associated with G108--S1 and G108--S2 are detected at all four bands of WISE (Figure 6).
Hereafter, the IR sources associated with G108--S1 and G108--S2 are called IRS 1 and IRS 2, respectively.
IRAS 22565+5839, an associated IRAS point source from the PGCC catalog, is located at the center of the projected separation of IRS 1 and IRS 2, suggesting that the IRAS source is resolved at the WISE 12 \micron\ with a higher spatial resolution ($\sim$6 \arcsec).
IRS 1 and IRS 2 are identified as YSO candidates based on the diagnostic color-color and color-magnitude diagrams (See Figure 11) in the YSO identification schemes presented by \citet{koenig14}.

The evolutionary stages of IRS 1 and IRS 2 are classified by their spectral indices and bolometric temperatures.
A spectral index $\alpha$ is derived by fitting the photometric data in the wavelength range from 2 to 24 \micron\ as the following \citep{evans09};
\begin{equation}
\alpha = \frac{d\ \textrm{log}(\lambda S(\lambda))}{d\ \textrm{log}(\lambda)}.
\end{equation}
Here, $S(\lambda)$ is the flux density at the wavelength $\lambda$.
The photometric data used to estimate the spectral index are listed in Table 2.
The spectral indices of IRS 1 and IRS 2 are 0.61 and 0.48, respectively.
Using the classification scheme from \citet{evans09} (i.e., Class I for 0.3 $\leq \alpha$, Flat for --0.3 $\leq \alpha <$ 0.3, Class II for --1.6 $\leq \alpha <$ --0.3, and Class III for $\alpha <$ --1.6), both are classified as Class I sources.

The bolometric luminosities ($L_{\textrm{bol}}$) and bolometric temperatures ($T_{\textrm{bol}}$) of the two YSO candidates are also calculated.
The $L_{\textrm{bol}}$ of IRS 1 and IRS 2 are 27 and 30 $L_{\sun}$, respectively, indicating these two sources are low-mass YSOs ($L_{\textrm{bol}} <$ 50 L$_{\sun}$).
IRS 1 and IRS 2 have $T_{\textrm{bol}}$ of 341 K and 614 K, respectively.
Following the classification criteria from \citet{myers93} (i.e., Class 0 for $T_{\textrm{bol}} < 70$ K, Class I for 70 K $\leq T_{\textrm{bol}} \leq$ 650 K, and Class II for 650 K $< T_{\textrm{bol}} \leq$ 2800 K), both are also classified as Class I sources.
The CO outflows, which are commonly associated with embedded Class 0/I sources, are not detected in these two Class I sources.
Higher resolutions and better sensitivities may reveal the associated outflows.
The bolometric luminosities, the bolometric temperatures, and the spectral indices of the two IR sources are listed in Table 3.

\subsection{Clump properties of G108--N and G108--S}

\subsubsection{Gas temperature}

We assume that the $^{12}$CO line is optically thick and all levels are in local thermodynamic equilibrium (LTE) to derive its excitation temperature \citep{liu13}.
Therefore, the excitation temperatures ($T_{\textrm{ex}}$) in all levels and the kinetic temperature ($T_{\textrm{kin}}$) are the same.
We also assume that dust and gas are well coupled ($T_{\textrm{ex}} = T_{\textrm{kin}} = T_{\textrm{dust}}$).

The excitation temperature is derived from the brightness temperature of CO 2--1, which is optically thick ($\tau_{\nu} \gg 1$).
The expression for the brightness temperature, $T_{\textrm{b}}$ is:
\begin{equation}
T_{\textrm{b}}=[J_\nu(T_{\textrm{ex}})-J_{\nu}(T_{\textrm{bg}})](1-e^{-\tau_{\nu}})f,
\end{equation}
where $J_{\nu}=h\nu_{\textrm{u}}/k(e^{h\nu_{\textrm{u}}/kT} -1)^{-1}$, $\tau_{\nu}$ is optical depth, and $f$ is the beam filling factor and assumed as unity.

We compared the calculated $T_{\textrm{ex}}$\ with the result of the previous studies.
The mean $T_{\textrm{ex}}$ toward G108--N and G108--S are 13.4 K and 12.5 K, respectively, which are consistent with the $T_{\textrm{dust}}$\ (11.9 $\pm$ 2.8 K) of PGCC G108.84--00.81\ from the Planck PGCC catalog \citep{planck15}.
$T_{\textrm{kin}}$\ from the ammonia observations \citep{tatematsu17} of G108--N and G108--S are 14.3 K and $<$ 19.1 K, respectively.
The calculated $T_{\textrm{ex}}$\ is also consistent with this $T_{\textrm{kin}}$, suggesting that our LTE assumption is reliable.

\subsubsection{H$_2$\ Column Density derived from $C^{\textit{18}}O$ 2-1 line}
We calculate the H$_2$\ column density from the C$^{18}$O line assuming LTE and the same excitation temperature as CO.
The column density, N$_{\textrm{thin}}$, under the assumption of optically thin emission ($\tau \ll$ 1) can be estimated with the integrated intensity of the line integral $W$ (K km s$^{-1}$) \citep{schnee07} as the following,
\begin{equation}
N_{\textrm{thin}} = \frac{8{\pi}W}{{\lambda}^{3}A}\frac{g_{l}}{g_{u}} \frac{1}{J_{\nu}(T_{\textrm{ex}}) - J_{\nu}(T_{\textrm{bg}})}
\frac{1}{1 - \textrm{exp}(-h{\nu}/kT_{\textrm{ex}})} \frac{Q_\textrm{rot}}{g_{l} \textrm{exp}(-E_{l}/kT_{\textrm{ex}})}\:\textrm{cm}^{-2}
\end{equation}
where $\nu$ and $\lambda$ are the frequency and wavelength of the transition, $A$ is the Einstein coefficient, $g_l$ and $g_u$ are the statistical weights of the lower and the upper levels, $J_{\nu}(T) = \frac{h{\nu}/k}{\textrm{e}^{h{\nu}/kT}-1}$, $Q_{\textrm{rot}}$ is the partition function, and $E_l$ is the energy of the lower level.
The energy of the each level is given by $E_{J}=J(J+1)hB$ where $B$ is the rotational constant.

However, in some cases, C$^{18}$O 2--1\ is not perfectly optically thin.
An optical depth can be corrected in the calculation of column density by using the correction factor, $C_{\tau}$, as long as $\tau \leq 2$ \citep{schnee07}.
\begin{equation}
C_{\tau}=\frac{\tau}{1-e^{-\tau}}.
\end{equation}
The optical depth ($\tau$) can be found from
\begin{equation}
\tau = -\textrm{ln}\left[1-\frac{T_{\textrm{thin}}}{J(T_{\textrm{ex}})-J(T_{\textrm{bg}})}\right],
\end{equation}
where $T_{\textrm{thin}}$ is the beam corrected brightness temperature of the given line.
The final column density corrected for the optical depth is
\begin{equation}
N=N_{\textrm{thin}} \cdot C_{\tau}.
\end{equation}

Finally, the H$_2$ column density is derived by dividing the abundance of the molecule $x$, $X(x)$:
\begin{equation}
N (\textrm{H$_2$}) = \frac{N(x)}{X(x)} \ \textrm{cm}^{-2}
\end{equation}
The C$^{18}$O abundance, $X(\textrm{C$^{18}$O)}$, of $4.8\times 10^{-7}$ is used \citep{lee03}.

The sizes of G108--N and G108--S are defined as $R=\sqrt{a\cdot b}$, where $a$ and $b$ are the major and minor axes of deconvolved FWHM size measured at the 50 $\%$ contours of the C$^{18}$O 2--1\ emission region.
The mean H$_2$\ column densities of G108--N and G108--S within the clump size are 6.7 $\times 10^{21}$ and 1.0 $\times 10^{22}$ cm$^{-2}$, respectively.
Derived parameters are listed in Table 4.

\subsubsection{H$_2$\ column density derived from dust continuum emission}

 The molecular gas column density can be calculated with the dust continuum flux, $S_{\nu}$, using
\begin{equation}
N(H_2) = \frac{S_{\nu}}{{\mu}m_{\textrm{H}}{\kappa}_{\nu}B_{\nu}(T_{\textrm{dust}}){\Omega}}\ \textrm{cm}^{-2}
\end{equation}
where $\mu$ is the mean molecular weight, $m_{\textrm{H}}$ is the atomic hydrogen mass, ${\kappa}_{\nu}$ is the mass opacity coefficient, and $B_{\nu}(T_{\textrm{dust}})$ is the Planck function with a dust temperature ($T_{\textrm{dust}}$).
The dust temperature $T_{\textrm{dust}}$\ is adopted from the gas temperature derived in Section 4.2.1.
The aperture solid angle, $\Omega=\pi\theta^2/4 ln2$ is a circular Gaussian aperture where $\theta$ is the beam FWHM.
We use the 850 \micron\ dust continuum emission to calculate the H$_2$\ column density.
The mass opacity coefficient of 0.018 ${\textrm{cm}}^2 \ {\textrm{g}}^{-1}$ \citep{ossenkopf94} is used, by assuming a gas-to-dust ratio of 100.
In order to make a consistent comparison, the 850 \micron\ data have been smoothed to the C$^{18}$O 2--1\ resolution.
A beam FWHM of 32.5\arcsec\ is used to calculate the aperture solid angle.
Within the clump size, the mean H$_2$\ column densities of G108--N and G108--S are 5.6 $\times 10^{21}$ and 8.4 $\times 10^{21}$ cm$^{-2}$, respectively.
Derived parameters are also listed in Table 4.

\subsubsection{Total mass and kinematics}
Dust continuum emission at 850 \micron\ is known as one of the best tracers of the total cloud mass because it is optically thin.
Therefore, we derive the total (gas+dust) masses, $M_{\textrm{total}}$, of G108--N and G108--S, using
\begin{equation}
M_{\textrm{total}} = \frac{S_{\nu}{d}^{2}}{{\kappa}_{\nu}B_{\nu}(T_{\textrm{dust}})},
\end{equation}
where S$_{\nu}$ is the 850 \micron\ integrated flux and $d$ is the distance \citep[3.21 $\pm$ 0.21 kpc;][]{ramirez11}.
We adopt the same coefficient as those used in Equation (8).
$T_{\textrm{dust}}$\ for G108--N and G108--S are adopted from the gas temperature derived in Section 4.2.1. as 13.4 and 12.5 K, respectively.
Their derived total masses are listed in Table 5.
The total mass of G108--N is larger than the sum of the masses of G108--S1 to S4; the total mass of G108--N is 386 $\pm$ 2 M$_{\sun}$, indicative of a massive starless clump.

To investigate whether the clump is gravitationally unstable, and thus, the possibility of future star formation, we compare its Jeans mass with the total clump mass.
The gas in molecular clouds is supported against gravitational collapse by turbulence and magnetic field as well as the thermal pressure.
The Jeans mass can be derived by
\begin{equation}
M_J \approx \left(\frac{T_{\textrm{eff}}}{10\:\textrm{K}}\right)^{\frac{3}{2}}\left(\frac{\mu}{2.33}\right)^{-\frac{1}{2}}\left(\frac{n}{10^{4}\:\textrm{cm}^{-3}}\right)^{-\frac{1}{2}} M_{\sun},
\end{equation}
taking into account the thermal and turbulent support \citep{hennebelle08}, where $n=N(H_2)/2R$ is the volume density of $H_2$.
The effective kinematic temperature, T$_{\textrm{eff}}$, is given by
\begin{equation}
T_{\textrm{eff}}= C^{2}_{s, \textrm{eff}}  {\mu}m_{\textrm{H}}/ k
\end{equation}
with the effective sound speed C$_{s, {\textrm{eff}}}$.
The C$_{s, {\textrm{eff}}}$ including thermal and turbulent support can be derived by
\begin{equation}
C_{s, {\textrm{eff}}}= \left[({\sigma}_{\textrm{NT}})^{2} + ({\sigma}_{\textrm{T}})^{2}\right]^{\frac{1}{2}}.
\end{equation}
The one-dimensional thermal (${\sigma}_{\textrm{T}}$) and non-thermal (${\sigma}_{\textrm{NT}}$) velocity dispersions can be calculated as follows,
\begin{equation}
{\sigma}_{\textrm{T}}= \left[\frac{kT_{\textrm{ex}}}{m_{\textrm{H}}\mu}\right]^{\frac{1}{2}}
\end{equation}
\begin{equation}
{\sigma}_{\textrm{NT}}= \left[{\sigma}^{2}_{\textrm{C$^{18}$O}} - \frac{kT_{\textrm{ex}}}{m_{\textrm{c$^{18}$O}}}\right]^{\frac{1}{2}},
\end{equation}
where $k$ is the Boltzmann's constant.
${\sigma}^{2}_{\textrm{C$^{18}$O}}=\Delta V^{2}_{\textrm{C$^{18}$O}}/8ln(2)$ is the one-dimensional velocity dispersion of C$^{18}$O 2--1\ and $m_{\textrm{C$^{18}$O}}$ is the mass of C$^{18}$O.
The calculated Jeans mass is 299 $M_{\sun}$ with $n=1.0\times10^3$ cm$^{-3}$, $T_{\textrm{eff}}=222$ K, $\sigma_{\textrm{T}}=0.20$ km s$^{-1}$, and $\sigma_{\textrm{NT}}=0.79$ km s$^{-1}$.
The total mass of G108--N (386 $M_{\sun}$) is larger than $M_J$, suggesting that G108--N is gravitationally unstable (i.e., a prestellar clump).

\subsection{Chemical status of two clumps}

\subsubsection{CO depletion}
According to the comparison between the integrated intensity distributions of molecular lines and dust continuum, the molecular line emission peaks are slightly shifted to SW from the dust continuum emission peak.
This might be caused by the molecular depletion at the dust continuum peak \citep{lee03}.
We compare the H$_{2}$ column densities, $N(\textrm{H}_2$), derived from C$^{18}$O 2--1\ and the 850 \micron\ dust continuum emission to derive the CO depletion factor, which is defined as:
\begin{equation}
D_{\textrm{co}}= \frac{N({\textrm{H}}_2)_{\textrm{dust}}}{N({\textrm{H}}_2)_{{\textrm{C}}^{18}{\textrm{O}}}}.
\end{equation}

The maximum depletion factor of G108--N is about 1.8 while that of G108--S is about 4.
The low CO depletion suggests that the dynamical timescales of G108--N and G108--S are not very large, that is, the high-density clumps might form recently.
However, we cannot rule out an artificial effect; the H$_2$\ column density derived from dust continuum emission could be underestimated because the extended structure is possibly filtered out during the reduction process.

\subsubsection{Molecular abundances}

Figure 12 shows the averaged spectra within the 50 $\%$ contour of integrated intensity peak of N$_2$H$^+$ 1--0\ towards G108--N and G108--S obtained with the NRO 45 m telescope; the N$_2$H$^+$ 1--0\ emission is spatially distributed in larger area than the beam FWHM (20.4 $\arcsec$).
The N$_2$H$^+$ 1--0\ line is fitted using the hyperfine structure (HFS) fitting method in GILDAS/CLASS to determine $T_{\textrm{ex}}$\ and optical depth, $\tau$.
In both clumps, the N$_2$H$^+$ 1--0\ lines are optically thin ($\tau < 0.1$).
Derived $T_{\textrm{ex}}$\ of G108--N and G108--S are 3.7 and 3.3 K, respectively, which are very low, compared to the $T_{\textrm{ex}}$\ of CO in G108--N (13.4 K) and G108--S (12.5 K).
We also derived the $T_{\textrm{ex}}$\ of HCN by fitting the HFS of the HCN 1--0\ line.
The spectra of HCN 1--0\ at each positions are presented in Figure 13.
The $T_{\textrm{ex}}$\ of HCN in G108--N and G108--S are 3.6 and 3.8 K, respectively, which are similar to those of N$_{2}$H$^{+}$.
The optical depths at all five positions are less than 1.

N$_{2}$H$^{+}$ and HCN seem sub-thermally excited, so we derive column density of N$_{2}$H$^{+}$ and HCN using a non-LTE radiative transfer code, RADEX \citep{vandertak07}.
We assume that $T_{\textrm{kin}}$\ is equal to $T_{\textrm{ex}}$\ derived from C$^{18}$O 2--1\ for G108--N and G108--S.
The mean H$_2$\ volume density is derived from the 850 \micron\ dust continuum emission.
For the N$_{2}$H$^{+}$ analysis, the 850 \micron\ dust continuum map is convolved with the beam FWHM of NRO 45 m.
The line widths of isolated component of N$_2$H$^+$ 1--0\ ($F_{1}, F=0,1 \rightarrow 1,2$) of 1.72 and 2.67 km s$^{-1}$ for G108--N and G108--S, respectively, are used.
Calculated N$_2$H$^+$ 1--0\ column densities of G108--N and G108--S are 1.2 $\times 10^{14}$ and 1.9 $\times 10^{14}$ cm$^{-2}$, respectively.
$T_{\textrm{ex}}$\ from non-LTE calculation are 3.1 and 3.0 K for G108--N and G108--S, respectively, which are consistent with the result from the hyperfine structure (HFS) fitting method.
The optical depth, however, calculated using non-LTE method are larger than that calculated by the HFS fitting.
Fractional abundance of molecule $x$, $X(x)$, can be derived as follows,
\begin{equation}
X(x) = N(x) / N(\textrm{H}_{2})_\textrm{dust}.
\end{equation}
The fractional abundances of N$_2$H$^+$ 1--0\ are 1.2 $\times 10^{-8}$ and 2.5 $\times 10^{-8}$ for G108--N and G108--S, respectively.
G108--N and G108--S have higher fractional abundances than previously studied dense cores ($X(\textrm{N}_{2}\textrm{H}^{+}) \sim 1 \times 10^{-10}$) by \citet{caselli02}, \citet{tafalla02}, and \citet{di04}.
On the other hand, the N$_2$H$^+$ 1--0\ fractional abundances of two clumps are consistent with those of cores within ``Clump--S" of PGCC G192.32--11.88 \citep{liu16}, which are calculated in the assumption of LTE.
The $T_{\textrm{ex}}$\ of cores in ``Clump-S" is about 5 K and the optical depths is about 4.
Derived parameters using N$_2$H$^+$ 1--0\ are listed in Table 6.

For the non-LTE analysis of HCN 1--0, the 850 \micron\ dust continuum map is convolved with the beam FWHM of KVN 21 m to derive the H$_2$\ volume desity.
The HCN 1--0\ spectra at the positions of the 850 \micron\ emission peaks are presented in Figure 11.
The line width of the strongest component of HCN 1--0\ is used.
We average the four values for G108--S1, S2, S3, and S4 as a representative value for G108-S for the consistency with the N$_{2}$H$^{+}$ analysis.
$T_{\textrm{ex}}$\ from the non-LTE calculation for HCN 1--0\ are 3.8 and 4.0 K toward G108--N and G108--S, respectively.
The column densities of HCN 1--0\ in G108--N and G108--S are 7.8 $\times 10^{14}$ and 6.5 $\times 10^{14}$ cm$^{-2}$, respectively.
The optical depth from the non-LTE method are larger than that from the HFS analysis.
The fractional abundances of HCN 1--0\ are 3.9 $\times 10^{-7}$ and 2.9 $\times 10^{-7}$ for G108--N and G108--S, respectively.
Derived parameters with HCN 1--0\ are listed in Table 7.

\section{DISCUSSIONS}

PGCC G108.84--00.81\ is located close to dynamically active regions such as an H{\sc ii} region (Sh2-152) and a SNR (SNR G109.1--1.0).
SNR G109.1--1.0 is located at the east of PGCC G108.84--00.81.
A line profile composed of two components, a sharp single peaked component with a broad component, was shown in the interacting regions between CO molecular clouds and SNRs \citep{seta98,su14}.
So, the association between SNR G109.1--1.0 and CO molecular cloud in the vicinity of the remnant has been previously investigated \citep{tatematsu87,tatematsu90}.
However, according to \citet{tatematsu90}, any broad CO emission, which is possibly accelerated by SNR G109.1--1.0, was not detected.

The channel map of CO 1--0\ line emission of PGCC G108.84--00.81\ are shown in Figure 14.
The CO emission distributes along two filaments.
A thin filament to the east is seen from --55 to --52 km~s$^{-1}$.
The main filament, which includes G108--N and G108--S, is seen from --52 to --46.5 km~s$^{-1}$.
The two filaments may be interacting in the north-east region, where IRAS 22576+5843 is located.
However, the broad CO emission, which could be a hint for the interaction, does not appear.
The thin filament is located in front of the main filament and seems to make a shield against the SNR shocks.
As mentioned in section 3.2, CO 2--1$/$CO 1--0\ ratios along the main filament are not enhanced by shocks.
Therefore, the main filament seems unaffected by the SNR.

However, the star formation in G108--S seems affected by the southern H{\sc ii} region, Sh2-152; G180--S is bent probably due
to external compression by Sh2-152 and the CO 2--1$/$CO 1--0\ ratio is enhanced at the bent region (see Figure 5).
The gravitational collapse and fragmentation of G108--S might be induced by Sh2-152.
G108--S is more evolved than G108--N.
G108--N is a massive prestellar clump while G108--S is fragmented into 4 cores  at least , G108--S1, G108--S2, G108--S3, and G108--S4, and G108--S1 (IRS 1) and G108--S2 (IRS 2) are associated with Class I sources.
The overall clump properties of G108--N and G108--S are similar, and their chemical status does not show significant difference; G108--S is slightly more evolved than G108--N in the view of CO depletion.

By comparing the pressures of G108--S and Sh2-152, one can investigate whether the evolution of G108--S has been affected by Sh2-152.
The internal pressure of Sh2-152 can be derived using \citep{morgan04}
\begin{equation}
\frac{P_{\textrm{H{\sc ii}}}}{k}= 2n_{\textrm{e}}T_{\textrm{e}}.
\end{equation}
The effective electron temperature $T_\textrm{e}$ is assumed to be $10^4$ K.
For the electron density, the peak value ($n_\textrm{e}=2000$ cm$^{-3}$) from \citet{heydari81} is used.
The derived $P_{\textrm{H{\sc ii}}}/k$ is $4.0\times 10^7$ cm$^{-3}$ K.
On the other hand, the molecular pressure inside G108--S is \citep{liu12a}
\begin{equation}
\frac{P_{\textrm{mol}}}{k}=nT_{\textrm{eff}}.
\end{equation}
The $P_{\textrm{mol}}/k$ is derived to be $7.3\times 10^5$ cm$^{-3}$ K with $n=4.5\times10^3$ cm$^{-3}$ and $T_\textrm{eff}=83$ K, which are obtained from the C$^{18}$O 2--1\ emission.
The pressure of Sh2-152 is two orders of magnitude larger than the internal pressure of G108--S.
It suggests that G108--S could be compressed by Sh2-152 if the two are physically associated.
More studies are needed to confirm whether the star formation in G108--S has been indeed induced by Sh2-152.
In contrast, G108--N is quiescent and seems unaffected by its surrounding environment yet.

The stability of G108--N was examined by comparing its total mass and the Jeans mass; the derived total mass is greater than the Jeans mass, indicating that G108--N is gravitationally unstable.
The free-fall time \citep[$t_{\textrm{ff}}=3.4\times10^7 n^{-0.5}$ yr,][]{evans99} for G108--N is about 1 Myr, which is similar to the typical lifetime of low mass starless cores with the average density of $n\sim10^{4}$ cm$^{-3}$.
The lifetime for massive prestellar cores is expected to be shorter than the free-fall time \citep{andre14}.
Therefore, G108-N might be about to collapse.
However, it is unclear whether G108--N will survive as a single massive prestellar core or be fragmented into several components as turned out in G108--S.
The peak surface densities of G108--N and G108--S are similar to 0.07 g cm$^{-2}$ as derived from the C$^{18}$O 1--0\ line.
The value is much smaller than the threshold surface density \citep[1 g cm$^{-2}$,][]{krumholz08} for fragmentation in massive star formation.
The estimated surface densities of IRDCs are 0.2 to 5 g cm$^{-2}$ \citep{battersby11}.
However, \citet{urquhart14} argued that adding the effect of magnetic field could reduce the threshold of surface density for fragmentation.
In addition, the distribution of surface densities of massive star-forming clumps shows that clumps with the surface density lower than 0.1 g cm$^{-2}$ can result in high mass star formation \citep[Figure 12 of][]{urquhart14}.
Therefore, we cannot exclude the possibility that G108--N could form a high-mass star without fragmentation.

\section{SUMMARY}

To investigate the star formation condition near active regions such as SNRs and H{\sc ii} regions, various molecular line observations as well as the submm dust continuum observation toward PGCC G108.84--00.81\ were carried out.
Our results are:

1. One filament structure presented in the integrated intensity maps of CO 1--0\ and $^{13}$CO 1--0\ is largely divided into three parts: the northeast region associated with a star, IRAS 22576+5843, the southern region directly linked to H{\sc ii} region, Sh2-152, and the central part defined here as G108 containing IRAS 22565+5839.
The two clumps, ``G108--N'' and ``G108--S'' are found within G108.

2. In G108--S, a blue-shifted component, whose velocity is similar to that of the component associated with Sh2-152,
is shown in both of the Moment 1 maps of CO 2--1\ and $^{13}$CO 2--1.
The integrated intensity ratio, $^{13}$CO 2--1$/$$^{13}$CO 1--0, is also the most enhanced at the southern edge of G108--S, which is close to the H{\sc ii} region.

3. Dust continuum emission also shows two components corresponding to G108--N and G108--S.
Highly fragmented structures in G108--S are revealed with the beam FWHM of JCMT/SCUBA-2 ($\sim14\arcsec$).
Four components, G108--S1, G108--S2, G108--S3, and G108--S4, are identified in the G108--S.
G108--N has no associated IR source, while there are two IR sources corresponding with the dust continuum emission peaks, G108--S1 and G108--S2.
The integrated intensity peaks of CO 2--1, $^{13}$CO 2--1\, and C$^{18}$O 2--1\ are slightly off that of dust continuum.

4. The HCO$^+$ 1--0\ and HCN 1--0\ show similar distributions to each other and also similar to the distribution of 850 \micron\ continuum emission
in G108--N.
The emission of two lines is distributed along the NE--SW direction with a cometary structure while HCO$^+$ 4--3\ is shown only in the head part.
This cometary structure is also shown in the integrated intensity map of NH$_{3}$ (1,1).
The centroid velocities of all lines are consistent.

5. IR sources, IRS 1 and IRS 2, associated with G108--S1 and G108--S2, respectively, are YSO candidates.
IRS 1 and IRS 2 are classified as Class I sources.
However, outflows associated with these Class I sources were not detected with our CO observations.
Higher resolutions and better sensitivities might reveal associated outflows.

6. The $T_{\textrm{ex}}$\ derived from CO observations of G108--N and G108--S are 13.4 and 12.5 K, respectively.
Total mass of G108--N is larger than the sum of total masses of G108 S1 to S4.
The total mass of G108--N is larger than the Jeans mass, suggesting that G108--N is a prestellar clump, which is gravitationally unstable and thus a potential future star formation site.

7. Two clumps have similar properties such as the gas temperature and the H$_2$\ column density.
Their chemical status does not show significant difference either although G108--N is slightly less evolved than G108--S in the view of CO depletion.

8. The gravitational fragmentation and star formation in G108-S seem induced by the compression from the H{\sc ii}, Sh2-152; G108--S is bent toward Sh2-152 and the CO 2--1$/$CO 1--0\ ratio is enhanced at the bent region.
In contrast, G108--N does not seem affected by its environment yet.

This work was supported by the Basic Science Research Program through the National Research Foundation of Korea (NRF) (grant No.NRF-2015R1A2A2A01004769) and the Korea Astronomy and Space Science Institute under the R\&D program (Project No. 2015-1-320-18) supervised by the Ministry of Science, ICT and Future Planning.
Tie Liu is supported by the KASI and EACOA fellowships. The James Clerk Maxwell Telescope is operated by the East Asian Observatory on behalf of The National Astronomical Observatory of Japan, Academia Sinica Institute of Astronomy and Astrophysics, the Korea Astronomy and Space Science Institute, the National Astronomical Observatories of China and the Chinese Academy of Sciences (Grant No. XDB09000000), with additional funding support from the Science and Technology Facilities Council of the United Kingdom and participating universities in the United Kingdom and Canada.
The KVN is a facility operated by the Korea Astronomy and Space Science Institute.

redpajama_set_name: RedPajamaArXiv


text:
Emitel S.A.
Cordiant Digital Infrastructure Limited
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Japan Medical Dynamic Marketing
Mitsui Chemicals
Advising Mitsui Chemicals, one of the largest Japanese chemical companies, on the acquisition of a 30% stake in Japan Medical Dynamic Marketing, a leading orthopedic medical device manufacturer in Japan, held by NGK SPARK PLUG
Netomnia
Avenue Capital, Advencap
Advised Netomnia, a UK-based fibre operator, on its first large-scale fundraise of £123m
Ferrovial Servicios
Portobello Capital
Advised Portobello Capital, a leading Spanish private equity firm with more than $1.75bn AuM, on the acquisition through a carve out process of a controlling stake in Ferrovial Servicios, a leading infrastructure service business in Spain owned by Ferrovial
Kao Data Ltd
Infratil Ltd
Advised Kao Data Ltd, which is jointly owned by Legal & General Group PLC and Noé Group subsidiary Hockham, on raising an initial £120m-£130m growth capital commitment from Infratil Ltd with the objective of creating a £500m data centre platform
Bitfield N.V.
Northern Data AG
Advising Northern Data AG, a Germany based developer and operater of high-performance computing ("HPC") infrastructure solutions, on the acquisition of Bitfield N.V., a company owning some 33,000 latest-generation ASIC miners
Faes Farma, flagship product Bilastine
Hikma Specialty USA INC
Advised Faes Farma in the signing of a long-term license agreement for its flagship product Bilastine with Hikma Specialty USA INC, a subsidiary of Hikma Pharmaceuticals PLC, for the United States of America
SiFi Networks America Limited (JV + 16.7% stake)
APG Group NV
Advising SiFi Networks America Limited, which provides open access fiber-to-the-home ("FTTH") networks across the US, on the sale of a 16.7% stake and establishing a joint venture with APG, under which APG will invest a $500m equity commitment
Decentric Europe BV
Advised Northern Data AG, a Germany based developer and operator of high-performance computing ("HPC") infrastructure solutions, on the acquisition of Decentric Europe BV, a company owning server systems with ~223,000 GPU cards, from Block.one
Pulsant Limited
Antin Infrastructure Partners
Advised Antin Infrastructure Partners on its acquisition of Pulsant from Oak Hill and Scottish Equity Partners. Pulsant is a hybrid cloud specialist, with a nationwide network of 10 data centres across the UK delivering secure, scalable and resilient cloud, colocation and networking services
SCG Packaging Public Company Limited
Advising Deltalab, a leading Spanish laboratory solutions provider with dedicated manufacturing capacity, on the sale of the company to SCG Packaging Public Company Limited, the largest integrated packaging and paper company in Southeast Asia
Portfolio of 16 European Consumer Healthcare brands from Sanofi
STADA Arzneimittel AG
Advising Sanofi, a leading global player in the Consumer Healthcare market, on the divestiture of a portfolio of 16 European Consumer Healthcare brands to STADA, a German pharmaceutical and consumer healthcare company owned by Bain Capital and Cinven
300 MWp solar PV portfolio in Iberia from Alten
Matrix Renewables
Advising Alten Energías Renovables ("Alten"), a global Independent Power Producer (IPP), on the sale of a solar PV portfolio of 300MWp in late stage of development across Spain and Portugal to Matrix Renewables, the renewable energy platform backed by global alternative asset manager TPG. In addition, Matrix Renewables and the Alten's Management Team have agreed to enter a Joint Development Agreement ("JDA") to further develop an additional 2GW of solar PV and storage assets across Iberia
Equiniti Group PLC
Siris Capital Group LLC
Advised Siris Capital, a private equity firm focused on the technology sector, on its recommended 180p cash offer for Equiniti Group PLC, a technology-led services and payments specialist
AtlasEdge Joint Venture
Liberty Global Inc., Digital Colony
Advised Liberty Global Inc., one of the world's leading converged telecommunication companies with operations in seven European countries, on the creation of AtlasEdge, a pan-European Edge Data Centre Joint Venture with the digital infrastructure investor Digital Colony
Bruc Energy, one of the largest renewable energy platforms in Spain with c.4 GWp of Solar PV assets under operation, construction and development
Universities Superannuation Scheme ("USS")
Advising Bruc OPT Energy Partners ("BROP"), a renewable energy JV owned by OPTrust and Mr. Juan Béjar, on the sale of a 50% stake in Bruc Energy, one of the largest renewable energy platforms in Spain with c.4 GWp of Solar PV assets under operation, construction and development, to funds managed by Universities Superannuation Scheme ("USS"), the largest pension scheme by assets in the UK
Whinstone Inc. – Subsidiary of Northern Data AG
Riot Blockchain Inc.
Advising Northern Data AG, a Germany based developer and operator of high-performance computing ("HPC") infrastructure solutions, on the sale of its U.S. subsidiary Whinstone Inc., an HPC data center operator based in Rockdale, Texas, to Riot Blockchain Inc., a U.S. based publicly-traded bitcoin miner
Acacia Pharma Group plc
Advised Acacia Pharma Group plc, a US headquartered commercial stage biopharmaceutical company incorporated in England and listed in Belgium, on its placing of 10m new ordinary shares at a price of €2.70 per share
Biogix, Inc.
Alliance Pharma plc
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Vorboss Limited
Fern Fibre Limited (Advised by Octopus Investments)
Advised Vorboss Limited, a London-based fibre operator, on its sale to Fern Fibre Limited / Octopus Investments, securing a funding commitment enabling an ambitious fibre deployment program
Kenedix
Sumitomo Mitsui Finance and Leasing
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Learning Materials for the K-12 Segment in Spain
Sanoma Oyj
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Axión Group
Asterion Industrial Partners
Advised AMP Capital on the sale of its portfolio company Axión Group, a leading independent broadcasting and telecommunications infrastructure provider in Spain, to Asterion Industrial Partners, a Spanish infrastructure fund
Cosmetic applications endolysin
Advised Micreos, a fast-growing biotechnology company, on a long-term license agreement with L'Oréal for one of Micreos' phage-based active ingredients, SA.100


Hansell MH, Ruxton GD, Ennos AR 2014. Collected and self-secreted building materials and their contributions to compression and tension structures. Biological Journal of the Linnean Society online.
Abstract. Animals that build structures have only two ways of obtaining their building materials: collecting them from the environment or secreting them. We identify a clear pattern among invertebrates: collected materials dominate in structures that bear loads predominantly in compression, whereas self-secreted materials dominate in structures that bear loads in tension. Among vertebrates, by contrast, structures in tension are much less common and may make use of either self-secreted or collected materials. Two possible explanations are examined for the difference between invertebrates and vertebrates. It may be that there has been evolutionary constraint on bodily secretions of vertebrates. Alternatively, the cost-effectiveness of self-secreted building materials diminishes with the load they bear in tension, and most vertebrates, because of their characteristically greater weight compared with invertebrates, exceed the viability threshold. Invertebrates have adapted biochemically varied secretions from a variety of glands to perform specialized mechanical roles. However, vertebrates have secretions with the potential to become building materials, in particular keratin, but only mucus-like secretions have evolved as building materials. The cost of suspended structures is predicted to become relatively greater with increased weight, whilst it will also become more difficult to find supports rigid enough to resist the forces they impose. This conforms to the relatively small size and small number of vertebrate structures in tension. The much larger, heavier suspended structures built by some social insects demonstrate that ecological factors may have important effects on the determination of weight thresholds.
In this paper weavers are refered to much as examples of nests in tension (suspended from above). Much larger birds would not be able to build hanging nests that were attached to thin branches, providing some safety from predators, as much larger nests would need thicker branches as support, and these nests would then be accessible to more predators.


text:
Michael Newman
Michael Newman is Jean Monnet Professor of European Integration Studies and Professor of Politics and he is also Course Leader of the BA in Peace and Conflict Studies. He is the Director of the London European Research Centre and is convenor of the European Studies subject group on the pan-European curriculum development project (the Tuning Project). His publications include Socialism and European Unity: The Dilemma of the Left in Britain and France, John Strachey, Harold Laski-A Political Biography, Ralph Miliband and the Politics of the New Left, and Socialism: A Very Short Introduction. His latest book, Humanitarian Intervention: Confronting the Contradictions will be published by C.Hurst and Co. in 2008.
Ralph Miliband and the Politics of the New Left
By Michael Newman January 2002
Ralph Miliband (1924-94) was a key 20th-century political thinker. His books The State in Capitalist Society (Quartet) and Parliamentary Socialism (Merlin) influenced a generation of the left and provided a focus for academic debate. Miliband's life and work were devoted to the attempt to define and apply an independent form of socialism. As a result of his published works, teaching and role in political movements, he became the most influential socialist political theorist writing in English, and he was as well known in North America, where he held several visiting professorships, as in Britain. His writings were also widely translated. The Socialist Register, which he founded (with John Saville) and edited for thirty years, brought him into contact with left-wing intellectuals throughout the world. Miliband, an energetic letter writer, corresponded on political issues with such figures as C.Wright Mills, E.P. Thompson, Leszek Kolakowski, John Saville, Marcel Liebman, Rossana Rossanda, K.S.Karol, André Gorz and Perry Anderson. Based on exclusive access to Miliband's extensive personal papers and supplemented by interviews, this book analyses the ideas and contribution of a key figure in the British and international Left from the second world war until the collapse of communism. It also provides an interpretative history of the evolution, debates and dilemmas of socialists throughout the period, and of the problems they faced both at work defending academic freedom and in society at large.


Lynsey Addario became a top photojournalist in the post-9/11 world. Her detention in Libya with 3 other New York Times journalists made international news. Addario's new book "It's What I Do" explains how she's negotiated difficult circumstances in Somalia, Afghanistan, Sudan, Iraq and countless other hot spots. The book offers an inside account of one of the world's most demanding jobs. Being in a male-dominated business, Addario negotiates the disadvantages of being a woman, while capitalizing on the advantages. She'll tell us about the professional and personal price of photojournalism today.


03 Sep, 2014 par F.P.
Lilou Mace is its name, is a refreshing to be infectious energy. In each of its views videos- thousands of times around the world do we perceive its contagious joie de vivre and his innate sense of sharing and exchange. Without a doubt, this superb French, 1m 81, born in Santa Barbara (California), an August 20, 1977, bears the stamp of service to others and actively contributes to the well being of humanity. She had the brilliant idea in 2006 to create his web TV. His unusual background and inspiring is to discover in our exclusive interview (1/2). In this new interview she talks about her spirituality (2/2).


You've got to have nothing but respect for Jim Furyk, who has played on every Ryder Cup and Presidents Cup team since 1997. If you've ever spoken to Furyk about these biennial matches, it's obvious that he truly cares about representing his country and enjoys the "team" aspect of these events.
Furyk was forced to withdraw from the last two FedEx Cup events due to a bone contusion on his wrist. He tried his best to rehabilitate the injury in time to compete in the Presidents Cup, but on Friday, he finally announced he would be unable to play. Instead, he'll travel with the team as an assistant to captain Jay Haas.
In the summer of 2004, Jason Day had breakfast sitting in the Lodge at Torrey Pines on Sunday before the final round of the Junior World Championships at Torrey Pines' South Course. He remembers not having an appetite because he was so nervous. At the end of that day, he hoisted the trophy and became the best amateur in the world. Eleven years later, Day found himself in a familiar setting, eating at almost the same table he did when he was 16, but as a golfer, he had matured with each year and he didn't have the same tense nerves this time around.
Heading into the week, Day had a feeling he was going to win this week. He told his wife Ellie that this year was different than the past seven years on the PGA Tour. They both have been expecting big things from Day, who was plagued with injuries last season, in 2015.
Harris English didn't have his A-game on Saturday at Torrey Pines, but he managed to escape with a one-over 73 in the third round of the Farmers Insurance Open and still shares a spot atop of a packed leaderboard.
English, who led by two heading into the weekend, got off to a nice start, making a birdie on the first hole to extend his lead to three shots. However, on a day with tough conditions at Torrey's South Course, he broke his streak of 39 holes with par or better on the par-4 6th. After driving it in the fairway bunker, he knocked his next shot short in the rough. His chip flew over the green and then he blew his putt to save par six feet past the hole before he missed the comeback for bogey and tapped it for a costly six.
On a gray, rainy morning at the Colonial Country Club in Cordova, a few miles northwest of Memphis, Jason Allred struggled his way through the back nine on the lengthy South Course. It was the first of two rounds he'd play as he attempted to nab one of the 13 U.S. Open spots in the Sectional Qualifier, competing with 145 other players to make next weekend's field at Pinehurst.


Zehner is experiencing rapid growth, and we are looking for a dynamic hands-on technology leader with ecommerce and management experience to join our team. We're seeking for a strong software architect, manager, communicator and someone that gets excited about taking teams to the next level. This role reports directly to the CTO and will partner closely with the larger executive team and other leaders across the company.
The ideal candidate will be an expert at software process and principles, but know how to be flexible to the rapidly changing nature of project in a digital agency. He/she will be a leader from the front, a coach and mentor to other team members. He/she will need to be an excellent communicator, know how to professionally interact and work with all other disciplines, including clients, business development, sales, project management, user experience and design.
Based in Los Angeles, Zehner is a full-service creative digital agency specializing in ecommerce for fashion & lifestyle brands. Services include digital & brand strategy, user experience design, technology selection & implementation, marketing, and post launch managed services. Our mission is to help our clients achieve their core business and ROI goals by crafting an engaging digital brand narrative. Founded in 2007, Zehner is now a strategic Shopify Plus partner, along with our key partnerships with Magento and Big Commerce. Our company culture is extremely important to us, and held together by our core values of: Relationships, Creativity, Exploration, Dedication, and Results. We embody the west coast LA lifestyle in everything we do, and we're proud of it.


TAO GROUP BLOG TAO NIGHTCLUB LAVO NIGHTCLUB TAO BEACH LAS VEGAS: TGIF! WHAT A NIGHT!
Last night was another memorable TAO night as we had special guests all over the club. Model Sarah Larson hosted the night, the Vegas girl arrived with 10 friends at 10pm. with a ton of press awaiting the local beauty she worked the carpet like a true pro. After dinner Sarah took over the Dancefloor VIP area by the owners table. Also coming in last night was American Idol and So You Think You Think You Can Dance star Nigel Lythgoe, who chose the more reclusive Skybox for his friends. Around 230AM TAO Regular Jamie Foxx joined us again taking over a dancefloor table and immediatley jumping on TAO's Catwalk with mic in hand to get the party going to the next level. Jamie MC'd the party for over an hour, having the club chant back to him, drinking Cristal and singing along with Hip hop classics spun by DJ REACH. Also, making a surprise appearance was actress Ashley Scott, who co-starred with Jamie in "THE KINGDOM". Ashley was celebrating her birthday and joined Jamie at his table fo a bit, he ofcourse bought her some Cristal for the occasion.


Communication with speakers of other languages has become much easier thanks to Translution's new Computer Assisted Translation (CAT) technology. The new software means that anyone wanting to write an email in English to work colleagues in France and Germany, for example, simply presses a button and the email will automatically arrive in the recipient's inbox, translated into their language. Similarly, incoming emails are translated into the user's own language or nominated language. The process is completely automatic and requires no special skill on the part of the user. Translution Pro gives users accurate, automatic translation of emails, attachments, documents and web pages instantly, without the need to cut and paste or to change ways of working. Also included are a set of tools which will dramatically improve the quality of the translation. Translution provides a service that for the first time will enable individuals and businesses to communicate and collaborate by email without language barriers, with improved translation quality. Translution consists of add-ins for Microsoft Outlook, Microsoft Word and Microsoft Internet Explorer and two standalone applications, Translution Control Centre (TCC) and Translution Dictionary Manager (TDM). The Outlook Add-in intercepts outgoing and incoming emails and determines if translation is required. It then redirects the emails to Translution Central for translation, translates them, and forwards them to the appropriate recipient. Emails can also be translated into multiple languages for multiple recipients automatically. Also, attachments can be automatically translated along with the Email. This process is undertaken without affecting normal working procedures and imposes no extra work.The add-ins to Word and Internet Explorer provide document and web page translations via processing by the Translution Central Site. With the Word Add-in you can translate sections of a document or an entire word document.
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Polite and well balanced preserves the unique and unmistakable profile of Lugana associated with freshness and greater organoleptic complexity resulting from its sparkling careful.
Produced with classic method sparkling wine with minimum of 15 months. It 's definitely the champagne most characteristic and typical of the area of Lake Garda. The sparkling base is obtained from a mixture of red grapes del Garda. These grapes are vinified with short maceration on the skins. You get a nice pink wine with a strong acid in order to better support the spumantizzazione.Questo sparkling wine is different from all the sparkling rosé. Surprise its scents of flowers and berries. Acidity discreet with a great freshness of taste sensations with an exceptional property.


A Report from Jaquai I have a ritual every year in which I go snowboarding on thanksgiving day, since I don't celebrate thanksgiving it gives me a nice diversion and the slopes are not as crowded as usual.
been doing it for many years now.
agian, as I had always had good shroom episodes.
air was still pretty crisp as we rode to the top of lift 1.
it was my first session of the season.


text:
Posted on June 5, 2014 by Rachael
After silence, that which comes nearest to expressing the inexpressible is music.
― Aldous Huxley
Today's Writing 101 prompt is to write about the three most important songs in your life. Well, true to my track record so far, I am not going to do that! For one thing, I find it impossible to choose just three songs. But I will say something about music more generally. Music is a big part of our family life. Both my children play piano to a high standard and they each have a second instrument, trumpet for my son and clarinet for my daughter. (She also plays the didgeridoo!) My daughter composes and recently she and a friend won a contest with a song they wrote and performed.
Not surprisingly for a photographer, I am a very visual person. I have no musical talent whatsoever but have often thought that of all creative endeavours, music is one of the most powerful in its ability to affect one on a visceral level. Darwin argued that music came before speech, and that feels right to me.
Now that I have two myself, I have been reminded that teenagers need music with the urgency of a biological imperative. Separate them from it for too long (say, more than five minutes) and they become quite incapable of coherent function. How and why, as we age, we become less dependent on music is beyond my ken. But when I rehear an old favourite song, after a long absence, I realise that music can still move me. It has the power more than any other thing to cut through the baggage of adult life and remind me what it was like to be that essential, earthy thing that is a teenager. I hope it always will.
Music was my refuge. I could crawl into the space between the notes and curl my back to loneliness.
This entry was posted in Music, photography, writing and tagged black and white, music, photography, teenagers, writing, Writing 101 by Rachael. Bookmark the permalink.
10 thoughts on "Music 101"
pianolearner on June 5, 2014 at 1:19 pm said:
It's never too late for you to start yourself….
J Bunnett on June 5, 2014 at 2:03 pm said:
Lovely studies. How many times did they have to play to get the shots?!
mvschulze on June 5, 2014 at 2:05 pm said:
Wonderfully said
I like your musical presentation… and what lovely kiddies you have!
oldshutterhand on June 5, 2014 at 10:00 pm said:
The dancing hands one is my favourite.
Helen Cherry on June 5, 2014 at 11:18 pm said:
Excellent.. I often cry when I hear music . love the Maya Angelou quote too.
Rachael on June 5, 2014 at 11:24 pm said:
Thanks, Helen. Seemed right to quote her now.
She was a real inspiration to me throughout her life.. as she was to many.
Love Happy Notes - Daily Fun and Inspiration on June 9, 2014 at 10:56 am said:
Such beautiful photographs and recognising the power of music. Great post. Thank you
dorothycunningham on July 3, 2014 at 12:56 pm said:


text:
Home > PODCAST > Interview and Podcast with Daso
Interview and Podcast with Daso
orn in Poona, India, Daso's first club experience goes all the way back to cruising around his daddy's disco's marble dance floor – on a floor polisher!
Now imagine this kid grown-up, having soaked up all kinds of musical influences on his "playground", from Miles Davis and Hendrix to the day-to-day hit machinery of contemporary radio pop: he became one of the most talented acts in the electronic music circus.
Daso's debut Daybreak (MBF Rec/2006) was released only one year after his move to Cologne: one of Germany's epicenters of techno culture.
Through the years Daso became a well-established act in the world of electronic dance music. He decided to take his next step and move to Berlin. After arriving in the capital of electronic dance music, Daso continued to release tracks through cutting-edge labels.
Above all, Daso is an extraordinary performer on a dandy level, with elegance and style.
How did you start in the electronic music businees? What drove you to make a career out of it?
Actually I did electronic music pretty early on. I learned it on the Atari ST of my dad when I was 12. I wasn't doing dance music in the beginning, but more more electronica and new wave. My first real inspiration came when I moved to Cologne and went to the clubs. It inspired me to write my first proper dance tracks. After doing that, I gave the cd to a friend in order to have a feedback. I never really thought about releasing it though. But he gave it to Riley Reinhold instead and I got a call that they want to release the track Daybreak on his Label MBF. After it got released, I got the news that I have a gig in 3 weeks. Yet, I didn't consider myself a Dj back then or a liveact artist yet, so I asked: "what should i do"? He told me there is a software called Ableton. You just need a laptop and a controller. So I bought a cheap laptop and learned the software in a short time and played my first gig.
I am on the road
since.
How do you prepare for a set? Do you think: I'm going to play these ten or twelve tracks or does it all happen on the spot?
I like to always try out clips of current projects or sketches into my sets and see people's reaction to it. The rest of the tracks revolve around my focus and mood of the moment.
So when was the last time you were nervous before a gig?
I don't remember when exactly, but one time I came for some reason 4 hours before my playtime to the club. And it seemed to not get crowded, so I got nervous. Because nobody likes to play before an empty club when you are the main act.
Did it live up to your expectations?
Luckily not. It became full in the last 20 minutes before I started playing and in the end it was completely packed. So I was really happy after all.
What would you recommend to the upcoming djs in cases which they are playing and a mistake happens for any reason?
I don't do big mistakes. But if there is a glitch in a set I think it is the best to keep calm and laugh about it. It is important not to get nervous and tense, otherwise you can ruin the whole mood of the party.
How do you find a balance in playing what you want to play and what people want to hear from you?
I think it is something you have to feel. In the beginning, I play some tracks and see what gets the crowd going. Only then, when I understand what makes them click, I manage to guide them a little. Nevertheless, I try to not get my ego in the way and just force it. They are here to have a nice night, not to be educated.
"Meine" definitely opened a lot of doors for me very fast.
As you come from Germany, could you please tell us if there are one or two German artists you would like to introduce us to?
Constanijn Lange is a guy you have to watch out for- very nice dreamy music, and I am planning a collaboration with Jonas Saalbach who is already a rising star in the biz and we gonna join forces soon.
But, I am really impressed with the Romanian producer scene, with guys like Cyclic's Gorje Hewek & Izhevski or BOg. I would also love to work with them.
The best club in the Germany (name and city)?
Berghain, Berlin
Your best souvenir of this summer: a place where you played for instance, or an anecdote?
It was on a beach in Goa. The place were I stayed was just 5 minutes from the Beach Club, so it was already dark and walked with my bag on the sand to the gig. Suddenly, wild dogs started running after me, so I had to constantly scare them off with the light of my mobile phone. It was a weird moment for me, but the gig on the beach was really amazing after all!
Tags	#interviews	#podcast	#Tech	#Tips	#Tricks
Interview with Aidan Doherty (WarmUp, London)
Interview and Podcast with Eran Aviner
Mix of the Day with Guhus
Interview and Podcast with Akira (Antwerp, BE)
Interview and Podcast with Gabriel Ananda
Interview and Full Premiere with Arjuna Schiks
Dreamer, 1 year ago 10 min read


Finding the right career can be a challenge for many adults with ADHD. Below is a link to an article that reviews many strategies one can employ to help people with ADHD find a career that is the best fit possible for them.
Find the article here at ADDitude Magazine.
Women and ADHD Do you have ADD/ADHD?


text:
Baseball Database
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Birth date 26 Apr 1992 (27 years)
Nationality United States
Nickname All Rise
Aaron Judge, formally known as Aaron James Judge, is a professional baseball outfielder born in the Linden, California. He plays for the New York Yankees of the MLB and is known as one of the largest players in the major leagues. Since his MLB debut in 2016, he has been on a roll, knocking down records of previous MLB greats as well as winning awards left and right. His current award being the American League Rookie of the Year for 2017 where he won by unanimous selection.
Judge was adopted by teachers Wayne and Patty Judge. They revealed his adoption to him when he reached the age of 10 years old. When he reached high school, he attended his local Linden High School where he became a three-sport star. Not only was he a great pitcher and first baseman for the school's baseball team, he was also the football team's wide receiver, and the basketball team's center. As a football player, he set a record of 17 touchdowns, led the basketball team in 18.2 points per game, and played a part in helping the Linden High School baseball team make it to the playoffs of the California Interscholastic Federation Division III. While he was being pursued by football recruiters for his college career, Judge ultimately preferred baseball. He enrolled at the California State University in Fresno where he played for the Fresno State Bulldogs baseball team. He was named Freshman All-American by Louisville Slugger, won the 2012 TD Ameritrade College Home Run Derby, and led the team in terms of home runs, RBIs, and doubles in his junior year.
It wasn't until 2016 when Judge made his professional debut at the MLB. He hit a home run on his first professional career at bat and would go on to enjoy a much decorated yet much deserved rookie season in 2017. He broke several records in the MLB including the record for home runs by a rookie. Since his professional debut, he has been named All-Star, managed to win the Home Run Derby, and won the AL Rookie of the Month for April to June and September. He won the AL Player of the Month for June as well as September. He is currently the AL Rookie of the Year for 2017.
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Aaron Judge Hailed American League Rookie of the Year
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Where would you rather pitch?
Number of votes: 737


Hi – I love your post. My name is Juan-Domingo Soto, 27, and I am currently working in a large multinational corporation looking to move into Social Development. I felt very much identified with your article and I would greatly appreciate any help/guidance you or someone you may know is able to provide on the topic.
Thanks Juan! Feel free to email us with any questions you have!


His skill has not changed.
I am a published author and frequent writer in archery periodicals. Would you like to write an article together?
I have experience with 1-on-1 coaching and seminars alike. Would you like me to run a camp at your club?
I created several archery products and brought them to market. Would you like to collaborate on a new one?


The pasta was perfectly aldente. Really good flavor, can't recommend it enough. Also it is a nice place with Italian Ambiente and pretty interior.
ottimo ristorante,piacevole atmosfera, deliziose polpette di tonno,tagliatelle di farro porcini e tartufo fuori menù,baccalà in guazzetto(migliore di quello in agrodolce). servizio perfetto!torneremo!
Is a very good place, I recommend it the food is delicious for me one of the best places in Rome, besides the service is great and the prices very fair.
Ottima cucina e personale davvero molto amichevole e cortese. Consiglio le polpette di tonno, il baccalà in agrodolce (con pinoli e cipolle rosse) e il crumble alle mele (delizioso).
The carciofi alla giudia (Jewish style artichokes) appetiser is really good here. It was a special if the day though, not everyday.
Lovely food and atmosphere. Friendly English speaking staff. Slightly hidden away, but well worth the walk away from the main roads.
Cozy place, kindly personal, nice interior. Tried beef stake and some glass-served wine — it was very good.
Great restaurant, great food, great personnel with very good recommandations!!!
I would definitely recommend the braised Veal! Absolutely delicious!
It is very good restoraunt! Menu is not very big, but all food is fantastic!
Ambiente aconchegante. Atendimento nota 10, comida excelente. Ótimo custo benefício. Media de 12 euros o prato.
Comida boa, vinhos bons e preços medianos. O único ponto negativo foi o atendimento. A comida veio e o vinho não, tivemos que pedir. Quando pedimos a conta ninguém trouxe, tivemos que pedir de novo.
Şarap soslu sığır eti çok başarılı. Kesinlikle denenmeli.
Bel locale, cucina di tradizione rivisitata in modo intelligente, servizio molto cortese. Consigliato.
Завтрак до 12:15, обед до 15:00. Порции огромные и все очень вкусно!
Guanciolo di vitella con gateau di patate! Meraviglioso!!
Great location to eat something before visiting the Vatican Museum and with good service , however, the food is below average for Rome.
Delicious pasta - cacio e pepe. Very good trippa. Friendly staff.
Ottimo! Locale curato, ricette semplici ma di gusto!
Рейтинг на Foursquare завышен. Размер порций никак не назовёшь «огромным» (как сказано в одном из отзывов). Да и обслуживание… Пытались нас посадить (в пустом ресторане) за столик для двоих втроём.
Работает в воскресенье (увы, у итальянцев запросто может быть закрыто в любое время или день). Острая паста (помидоры, чеснок, перец) интересна, но порции не большие. Вино дорогое.
Wine and pasta, especially carbonara.
The beer selection was great.
Ispanaklı raviolinın tadı güzel ama doymak için değilde başlangıç olarak deneyin derşm.
Consigliato, cucina ottima e cortesia.
Cucina Romana... Si mangia molto bene e personale molto cortese.
Прекрасная кухня с типичными для региона Лацио блюдами. Хорошее обслуживание и виды на Ватикан.
"Small servings. Don't be fooled by the price... Perhaps it will be better ordering Italian food than being adventurous to try the steak and the fried chicken..."
"Try their special pasta, tonnarelli with chicory and pecorino cheese. Outstanding!"
"I love the aperitivo , excellent selection of food and the smoothies are fantastic"
"ใครชอบ Art หลงไหล Michalangelo หรือชอบดู Angel and Demon ใช่เลย กลับบ้านมาดูทันที"
"Good atmosphere. Lots of energy. Loved it there. Sit at a restaurant with a glass of wine and just enjoy the surroundings"
"Wonderful Square. Very impressive architecture. A Rome must see"