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Slope Interview Series: Rae Dinh, Unusual Ventures
By: Karine Hsu
Rae Dinh: Unusual Ventures
Content creation—from blogs to social media to email newsletters—is a vital part of any businesses' growth strategy. At Slope, we're focused on the intersection of brand + design, and our interview with Rae helped uncover how successful startups integrate strategic content with these other two focal points. Rae Dinh is the Director of Community and Content at Unusual Ventures. She leads content initiatives like the Field Guide and other programs at Unusual, including their Academy, Product Leaders Network, and Insights Series.
In this interview, Rae talks about various trends across different content channels, the major mistakes companies should avoid when ideating a winning content strategy, and how to create content that drives your brand's narrative forward.
For people that don't know you, talk briefly about your background. How did you wind up doing what you do? Describe your work as Director of Community and Content at Unusual Ventures.
Throughout college, I interned at a number of different startups (brands like Zola, Persado, and others). I also spent a summer working as a tech journalist in Israel at a media outlet called NoCamels, reporting on Israeli startups. It was a great experience, but I discovered that journalism wasn't for me. After graduation I worked at a tech policy think tank in Washington, D.C., and the World Economic Forum on their tech industry team. Eventually, I decided to get my graduate degree at the Oxford Internet Institute, which specializes in studying how we live online and researched major trends in online dating for my thesis.
After I graduated from Oxford, I worked as a Program Lead at the Partnership on AI, where I led our work around AI, Labor, and the Economy and was eventually recruited to be Director of Community and Content at Unusual Ventures. If I were to say there's a common thread, it would be that my work has consistently centered around technology and human behavior and storytelling around how the two intersect.
Talk a little bit about the different content streams/channels at Unusual, specifically the Unusual Field Guide and Unusual Academy.
We think of our Academy as a sort of "grad school for entrepreneurs," where we bring in industry experts who teach about the six common challenges that enterprise and consumer startups typically face in the earliest stages. The Academy itself is six weeks, typically in-person but we're running a virtual version for the first time this year. We also run programs for emerging Angel Investors (our Angel Academy) and a Product Leaders Network for exceptional product operators. A ton of our content draws from these programs and the amazing community of experts we've grown.
As far as content goes, our "bread and butter" is company-building content. My work specifically focuses on working with our team at Unusual to create tactical guides that are informative and immediately actionable. We just launched our Field Guide in April, and are humbled by the positive feedback we've received from entrepreneurs and others in our community. So overall, my content work revolves around gleaning insights from our community and sharing them via guides, events, etc., for our readers.
One of the most important things about our content strategy is the community aspect. Our community of experts and founders is where we draw our content from and helps give us continuous feedback on what's working and what isn't. That largely manifests itself in our programming, but also encompasses our growing online community. Lots of companies are trying to crack how to build organic communities around their brand and product, and content is a super important pillar of building a strong online community.
In terms of content creation, what are some of the biggest mistakes you see companies making? What are some of the most important lessons or principles around content creation that more brands need to understand?
One of the biggest mistakes I consistently see is brands pushing content that's too surface level or that adds little to the discussion.
"Just "putting something out there" isn't the same as creating quality content. Just like most professions, there's a huge difference, in my experience, between the highest level of quality content versus most of what you can find out there."
One tip I've tried to internalize is from Head of Marketing at Notion, Camille Ricketts, who said that content must either be highly tactical and immediately applicable, or it has to resonate emotionally with your audience.
Content that does neither of these two things really won't make a difference for your brand.
The biggest principle that content creators need to remember is this: know your audience, respond to them, and write content that either sparks feeling in them or helps them get their job done. I've never been a founder myself, so I talk to people who have founded companies or who have been in the trenches in the earliest stages to share content that is meaningful with our community and to receive feedback on content we're working on to make sure it will resonate with other entrepreneurs.
"One last thing: Have an authentic voice. Authenticity always wins when it comes to content. If you don't have that, you'll sound like everyone else and get lost in the noise."
Name your top companies doing really interesting, novel work around content. Are they experimenting with different mediums? Different tones? Visuals + copy?
Notion and Substack are two companies that immediately come to mind. Notion in particular has fostered a community that loves to share with each other (best tips, what they're learning, etc.), and how they use Notion to support that learning. Their content really helps create a vibrant community and vice versa.
Steezy is an Unusual portfolio company and actually had its roots as a content company, where it started off as a blog providing really valuable, unique content that catered to the dance community. They've grown into a platform where anyone can learn how to dance through really beautiful, well-produced videos. Lastly, I've been really impressed with Brightland and how prolific they've been around a simple topic like olive oil. You'll notice that all these companies have a stake in the ground and are mission-oriented companies -- and you can feel that in their content.
How do you think about the role that design plays when creating content? How do you think about the branding and design language behind each individual content initiative — how to keep it unique and interesting while still living under the umbrella brand of Unusual?
Design plays a huge part in our content creation process. We worked with a great design firm to build the Field Guide from the ground up to capture the look and feel of the entrepreneurial journey and this metaphor of climbing a mountain (culminating in founders raising their Series A). The Field Guide itself was also intentionally designed to feel like an e-learning center (think: LinkedIn Learning or Udemy/Coursera), rather than just a static blog. The goal there was to make sure busy founders could directly jump into the chapters that were relevant to them, versus having to read everything in order like a book. Once again, everything was designed with our core audience of early-stage founders in mind. It's reflected in the content we produce, all the way through to the way we deliver it.
Let's Chat: hi@slope.agency


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McConnell warns Dems would 'run roughshod' over country by changing Senate rules
Eliminating filibuster, packing courts and more would be on Dems' agenda, McConnell said
By Tyler Olson | Fox News
Sen. Manchin: I do not support getting rid of the filibuster and Chuck Schumer knows that
Democrat Sen. Joe Manchin says Joe Biden has a record of working well with Republicans and would work very well with the Senate as president.
Senate Majority Leader Mitch McConnell warned on Tuesday that if the Democrats win the Senate in November that they will change the rules of the chamber so that they can "run roughshod over the country" -- stark comments that came on the same day multiple Republican senators opined on protecting Senate norms.
"I think the American people should know what it means if the Senate shifts control, and you've heard it," McConnell, R-Ky., told reporters at the Capitol. "Eliminating the filibuster, D.C. statehood, Puerto Rican statehood, and packing the courts. That's what you get if you change the Senate."
If Washington, D.C., and Puerto Rico become states, they would each get two U.S. senators, adding four legislators who would almost certainly be Democrats to the 100-member body.
He added: "Who do they want to run the Senate? Do [voters] want to enable the Democrats to run roughshod over the country by changing the basic structure here? ... What [Democrats are] saying is they don't want to win the argument, they want to change the rules in order to guarantee the outcome, and I think the American people need to be aware of that before they vote on Nov. 3."
BIPARTISAN LAWMAKERS OFFER CORONAVIRUS RELIEF SOLUTION IN EFFORT TO BREAK LOGJAM
McConnell wasn't the only Republican senator to raise procedural concerns on Tuesday. Another was Sen. John Thune, R-S.D., who cited reports that some Democrats are setting up a strategy to get rid of the filibuster if Democrats win the presidential election and take control of the Senate. He pointed out that Democrats have filibustered multiple bills in recent months -- including the GOP's "skinny" coronavirus proposal last week.
"So the very mechanism that they used repeatedly here in just the last year ... they are now talking about getting rid of that very rule. Think about that. The irony of that is pretty rich," Thune said.
He continued: "Now the filibuster rule could be said to be the thing that distinguishes the Senate from the House of Representatives. That matters because the Senate is supposed to be different from the House of Representatives... The framers of the Constitution designed the Senate to be ... the cooling saucer of democracy. ... As time has gone on the legislative filibuster is the Senate rule that has had perhaps the greatest impact in preserving the founders' vision in the Senate. Thanks to the filibuster it is often harder to get legislation through the Senate than the House. It requires more thought. More debate."
Sen. Lisa Murkowski, R-Alaska, also chimed in, worrying about "efforts on the outside of this body that would ... push us to change our rules and do so in a way that could permanently erode and undercut the ability of the United States Senate to operate as intended."
SENATE FAILS TO ADVANCE 'TARGETED' $300B CORONAVIRUS BILL; RELIEF IN LIMBO
Sen. Dick Durbin, D-Ill., shot back that the Senate with the filibuster does not appear to be functioning as intended.
"I have to ask them in all candor, as I listened to the speech about preserving the Senate as we know it, if they are really taking a look at the Senate as we know it?" Durbin said. "Do you know how many amendments were debated on the floor of the United States Senate in the year 2019? In the entire year? The world's greatest deliberative body considered 22 amendments in the year."
Some moderate Democrats -- including West Virginia Sen. Joe Manchin -- have come out forcefully against getting rid of the filibuster.
The Senate on Tuesday also moved to confirm three U.S. District Court judges in California with overwhelming bipartisan support. McConnell made sure to emphasize in comments to the press that the votes were in keeping with the body's "blue slip" tradition in which district judges are approved by the senator of the state in which they are being nominated.
"You'll notice we've been confirming district judges on a bipartisan basis and I want to make the point that that underscores, that we are continuing the process of honoring the blue slip. There are 47 Democrats in the Senate each of whom would have the ability to block a judicial appointment from their home states," McConnell said. "And so we've continued to deal with district judges in the way they've historically been dealt with which is that the home state senator has a lot to do with it."
The Senate confirmed Mark C. Scarsi to the Central District of California 83-12, Stanley Blumenfeld to the Central District of California 92-4 and invoked cloture on Todd Wallace to be a judge for the Southern District of California 83-13.
McConnell has been the subject of criticism in the past because he has advanced federal appeals court nominations without blue slips. California Democratic Sens. Diane Feinstein and Kamala Harris specifically have attacked McConnell and Senate Republicans for this after they moved forward nominations to the 9th Circuit Court of Appeals over their objections. McConnell said Tuesday the circuit-level blue slip "has been on and off forever, but at the district level it remains uncharged."
Progressive activists have pressed Feinstein, who would likely take over the Senate Judiciary Committee if Democrats win the Senate, to abandon blue slips altogether. Feinstein has not taken a hard stance, according to the Los Angeles Times, on what she would do with blue slips for either circuit or district nominees -- though she warned, "what's sauce for the goose is sauce for the gander." She, like McConnell, is an institutionalist who has long supported the blue-slip practice.
Fox News' Chad Pergram contributed to this report.
Tyler Olson covers politics for Fox News Digital. You can contact him at tyler.olson@fox.com and follow him on Twitter at @TylerOlson1791.

redpajama_set_name: RedPajamaCommonCrawl


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Sødring Vildtreservat er et vildtreservat, der ligger ved udløbet af Randers Fjord og et område op langs kysten til udløbet af Mariager Fjord.

Et område på 38 ha strandenge med tidevandsrender, som kaldes loer, blev fredet i 1978. I 1999 udlagde Miljø- og Energiministeriet det kystnære havområde til vildtreservat, et areal på i alt 2.255 ha fordelt på 25 ha på land og 2.230 ha i havet. Det bedst beskyttede område er de små holme Mellempolde ved udløbet af Randers Fjord, hvor der er færdsel forbudt fra 1. april til 15. juli af hensyn til ynglende kystfugle. I resten af området er jagt og brætsejlads forbudt i den sydlige del af reservatet ud for Sødring, mens der er forbud mod motorbådsjagt og opsøgende jagt i den øvrige del.

Eksterne kilder/henvisninger
Naturstyrelsens folder om reservatet

Fredede arealer i Danmark
Vildtreservater i Danmark
Randers Kommunes geografi
Randers Fjord

redpajama_set_name: RedPajamaWikipedia


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Settle Covid-19 Insurance Claims within 3 Days: Finance Ministry
December 4: The Ministry of Finance has directed the Insurance Board to facilitate in settlement of claims related to coronavirus within three days.
The finance ministry reportedly issued a fresh call to the Insurance Board following complaints that the beneficiaries were not receiving compensation or were facing hassles despite the government's clear instructions to release the amount to those who meet all the criteria.
Earlier on November 3, the finance ministry had instructed the board to settle such claims within seven days.
The ministry noted that only a handful of cases have been settled so far and the board has also failed to present daily progress report to the ministry regularly.
According to the state-run national news agency (RSS), the ministry has instructed the board to ensure that the applicants who fulfill all the criteria related to coronavirus insurance claims must receive the compensation amount within three days and the report must be submitted to the ministry on a daily basis.
The ministry has also directed the concerned authorities to complete the verification process as soon as possible, RSS reported.
The board has also been directed to publish the details related to coronavirus insurance including the verifications done so far, number of claims settle till date, related documents, false claims among others.


In 2006 we invented the Alternative tours concept in Berlin to show other responsible, respectful and open minded people the raw and artistic side of this great city. To support the places we love and which we felt needed our help before they were swallowed up and changed forever.
With an extensive connections to associations, organizations, local business', artists, crews, collectives etc. it is our aim to give you unique experiences and superb value for your time and money.
We have an in-depth and personal understanding of the places, people and Berlin´s art scenes, offering our tours to individuals, companies, students and special interest groups on a daily basis for the past 10 years. We are also proud to be a sponsor of various projects, events and initiatives in the local community. Unlike other imitators who see our Alternative tours as a new fad to cash in on, we live and breathe this stuff and we are in it for the long haul. No guide books or anyone for that matter can take you as close to the action as we can.
Our commitment to safe, responsible underground tourism is a top priority and we hope you will respect our ideals and contribute in some way to the vibe of these places you visit. You'll meet some wonderful personalities and gain some unforgettable life experiences on our tours and activities. So be adventurous and experience Alternative Berlin with us!
Tram: M2, M10 Prenzlauer Allee/Danziger Str.


Shop our wide selection of new ikan video heads. As an Authorized iKan Dealer, enjoy all of the benefits of manufacturer support from District Camera, your trusted source for the best iKan Video Heads like the IKan E-Image GH03 Fluid Head with Flat Base OR the newest products that were just released like the IKan E-Image GH03 Fluid Head with Flat Base. Are you shopping for Video Heads or Tripod Heads other than iKan? District Camera has you covered. Since 1978, casual photographers, students, semi-pros and serious photography professionals have trusted District Camera for our expert staff, selection, great prices and fast shipping.


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Home»World Records»Largest dinosaur footprints
Largest dinosaur footprints
Kids4Fun July 30, 2017	World Records Leave a comment 913 Views
Dampier Peninsula, Australia – July 28, 2017 – A team of palaeontologists from The University of Queensland and James Cook University has found some giant dinosaur footprints in northwestern Australia, measuring nearly 5 feet 9 inches in length, which sets the new world record for the Largest dinosaur footprints.
Photo: The biggest dinosaur footprint ever found, measures at about 5 feet 9 inches. A Team of paleontologists from the University of Queensland and James Cook University discovered 21 different types of fossils in area dubbed, 'Australia's Jurassic Park'
The Guinness World Records world record for the smallest dinosaur footprint discovered to date measures just 1.78 cm (0.7 in) from the heel to the tip of digit III. it was discovered on the Isle of Skye, Highland, UK by Dr Neil Clark (UK) of the Hunterian Museum of the University of Glasgow, UK, and announced in June 2004.
Guinness World Records also recognized the world record for the tallest mounted dinosaur skeleton; it is that of the Brachiosaurus brancai, which measured 13.27 m (43 ft 6 in) high on 1 June 2007.
A team of palaeontologists from The University of Queensland's School of Biological Sciences and James Cook University's School of Earth and Environmental Sciences braved sharks, crocodiles, massive tides and the threat of development to unveil the most diverse assemblage of dinosaur tracks in the world in 127 to 140 million-year-old rocks in the remote Kimberley region of Western Australia.
The footprints, which belonged to a long-necked herbivore called a sauropod, were found by a team of palaeontologists from The University of Queensland and James Cook University.
The research has been published as the 2016 Memoir of the Society of Vertebrate Paleontology.
The tracks were one of 21 specific track types, representing four main groups of dinosaurs, found in the 16-mile stretch of the Dampier Peninsula coastline, dubbed "Australia's Jurassic Park."
In a press statement, the study's lead author Steve Salisbury said that the area holds the most diverse collection of dinosaur tracks in the world, amounting to the "Cretaceous equivalent of the Serengeti."
"Among the tracks is the only confirmed evidence for stegosaurs in Australia. There are also some of the largest dinosaur tracks ever recorded. Some of the sauropod tracks are around 1.7 m long."
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Original Contributions| December 01 1968
Effect of Porcine Proinsulin in Vitro on Adipose Tissue and Diaphragm of the Normal Rat
Walter N Shaw, Ph.D.;
Walter N Shaw, Ph.D.
Biochemical Research Department, Lilly Research Laboratories, Eli Lilly and Company
Ronald E Chance, Ph.D.
Presented in part at the Twenty-eighth Annual Meeting of the American Diabetes Association in San Francisco, California, on June 16, 1968.
Diabetes 1968;17(12):737–745
https://doi.org/10.2337/diab.17.12.737
Walter N Shaw, Ronald E Chance; Effect of Porcine Proinsulin in Vitro on Adipose Tissue and Diaphragm of the Normal Rat. Diabetes 1 December 1968; 17 (12): 737–745. https://doi.org/10.2337/diab.17.12.737
The effect in vitro of porcine proinsulin and single component porcine insulin on the epididymal adipose tissue and the isolated diaphragm of the normal rat has been investigated. Both proteins enhance the oxidation of labeled glucose to carbon dioxide and its conversion to fatty acids by adipose tissue as well as glycogen formation from glucose by the hemidiaphragm. Kunitz pancreatic trypsin inhibitor (KPTI) but not the purified Kazal or soybean trypsin inhibitor block these effects of proinsulin on adipose tissue and diaphragm. KPTI has no effect on the response of these tissues to the single component insulin. Anti-insulin serum blocks the response of both adipose tissue and hemidiaphragm to proinsulin and single component insulin. The enhancement of the oxidation of carbon one of glucose to carbon dioxide by adipose tissue in the presence of proinsulin is also blocked by KPTI.
It is concluded that porcine proinsulin itself cannot affect the glucose metabolism of adipose tissue and hemidiaphragm of the normal rat. Proinsulin exerts the biologic effect seen in this study because it is converted by an enzyme or group of enzymes present in adipose tissue and diaphragm muscle, to a molecule which is similar to or identical with insulin.


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Congressional Information
Laws & Statutes
US Code (USC)
Types of Legislation
There are four types of legislation - bills, joint resolutions, concurrent resolutions and simple resolutions. It is important to note that though there are thousands of bills introduced every year, very few actually make it all the way through the process and get enacted into law. Any bills or resolutions not enacted into law by the end of the of a Congress die and have to be reintroduced in the next Congress if sponsors want to try again. Remember, just because the name of the bill says ACT in the title, doesn't mean it actually made it through the process.
Bills are the usual form through which legislation is proposed.
Joint Resolutions, equivalent to bills, usually are for more limited matters such as constitutional amendments and money.
Concurrent Resolutions express facts, opinions, principles or purposes and are passed by both chambers (House and Senate).
Simple Resolutions are only considered in one chamber and are usually for procedural matters.
The Library of Congress has a nice overview of the legislative process on their new site Congress.gov. For more information, see:
How Our Laws Are Made
If a bill or resolution passes both chambers it then goes to the President for approval. If the President vetoes a bill it takes votes of two-thirds of both chambers to override it before it can be enacted. Enacted bills are published in the Statutes at Large. See the Laws & Statutes tab for more information.
Finding Bills and Resolutions
Here are some of the best locations for finding bills and their status.
Congress.gov - you can search the full text of legislation by words, phrases or bill numbers. This site will also allow you to search bill summaries and status, browse or search multiple Congresses.
American Memory Bills and Resolutions (Library of Congress) - available for selected sessions beginning with the 6th Congress for the House and the 16th Congress for the Senate.
Contains all published versions of bills. Browse by category to find bills and regulatory information, or search for specific documents.
If you want see how a particular member of Congress or a particular party votes on major bills or other vote statistics you will need to look at the Roll Call of votes. This is usually listed by the Congress/year, bill number, member's name and party. Sources for Roll Call votes includes:
The US House Roll Call Votes site provides voting information from the 101st Congress, 2nd Session (1990) to the present.
The US Senate Roll Call Votes site provides access from the 101st Congress (1989) to the present.
The Congressional Record provides some copies of bills and roll call votes. We have access to the Congressional Record through several sources. The ProQuest Congressional database has the entire run including its predecessor.
Congress.gov [2011 - present]
ProQuest Congressional [1833- present] - this is available to NPS personnel only
Other sources include:
Congressional Votes Database (GovTrack) [1789 - present]
U.S. Congress Votes Database (Washington Post) [1991 - present]
Government information. Bills & statutes, budget & presidential materials, congressional committee materials, congressional rules & procedures, directories of organizations & officials, executive agency publications, judicial publications, legislate agency publications, proceedings of Congress & general congressional publications, regulatory information
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Last Updated: Sep 18, 2020 6:35 PM
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Subjects: Congressional Information
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And so a new year begins. Seasons greetings everyone. Hope you had some rest over December and feel refreshed and ready to take on a new year.
I've had a lot of time to think over the past month doing all the things I love – roadtrips, the bush, the sea, animals, friends, family, gardening, cooking, laughter, tears, movies, good food, good drinks, good books – thinking about the world and what I want for my life. 2013 was a big personal growth year for me with many ups and downs in the process. It didn't start or end the way I expected.
The world has been going through just as many ups and downs hasn't it. There's an almost palpable change in the way people are thinking – for the better I think.
Lately I've been thinking a lot about all the hundreds rules and regulations we all have to live by and impose on each other, and I find myself asking – why? And how?
There are 7.2 billion people on the planet. No two are alike. No two look the same. No two have the same outlook on life. No two have the same dreams. No two have the same insecurities. No two have the same wants. No two have the same personalities. No two have the same fingerprints!
There might be similarities, but not exacts. Which begs the question – by what and who's rules and regulations should we be living by and why? Why do we need to be 'ruled' in the first place? Who is it we are supposed to look like to be 'the ideal' when there are 7.2 billion different bodies and faces?
It is abundantly clear that none of the global economic, financial, governmental, social or religious systems currently in place on earth are working – and when you look at the variety of people on the planet, is it any wonder?
There is so much judgement, hate and anger in the world because we see ourselves as separate from each other, "us" against "them". We believe there is not enough of anything so we must fight to the death for our share.
What if all these assumptions are wrong? What if we've got it all wrong? What if the stories we've been told are incomplete?
We have no right to judge or rule any other. We came here to experience variety, joy and love. How about we let people experience what they want to without telling them they can't. Can't by who's estimation when there are 7.2 billion different ideas about how the world should work? If you don't like it, don't do it or don't look; but we can't stand in judgement of what other people want to experience. There is no right and wrong because we cannot know what any person's journey is inside – there are only choices.
We need more compassion, love and understanding in the world. Instead of pointing fingers at another, how about we point fingers at ourselves and look inside to see why what we viewed made us so angry. Each and every one of us is responsible for our own happiness. When we get infuriated by something 'out there', it is not that thing that is the problem, it is something inside of us we are denying.
But instead we blame, break, strike out and hurt people when all we are is scared to death and feel so utterly alone. We don't want our stories challenged and we're greatly threatened when they are. We take action when we are angry and vengeful which only compounds the problem instead of getting to a place of peace, understanding and acceptance first and reacting from there. Why?
What if there was nothing to be afraid of; what if we are never alone? Will we have the courage to look deep inside ourselves instead of judging others?
If we truly knew who we were, we would never harm another; ever. And we would know that there is enough of everything – love, money, resources.
Thanks love. Good to be back. Wishing you every success this year hun.
Welcome back, Veronique and Happy New Year!
Good words and advice for 2014.


Second annual 'Home Run for Health' planned for May 3 – San Bernardino American News celebtates 50 Years!
Residents and baseball fans throughout the Inland Empire are invited to hit a "Home Run for Health" May 3 when the Inland Empire 66ers face off against the Lake Elsinore Storm.
Riverside University Health System – Public Health, the San Bernardino County Department of Public Health, and the California Health Collaborative – Tobacco Control Program are teaming up again to share positive health messages while enjoying America's favorite pastime.
Fans are invited to pick up vouchers – while supplies last – for free admission to the May 3 game, when the 66ers host the Storm at San Manuel Stadium, 280 South E Street in San Bernardino. One voucher can be redeemed for four tickets and families are limited to two vouchers, for eight tickets total. Parking is $7 per vehicle and can be paid in credit or cash.


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Blog June 15th, 2021
The Value Of A Vehicle Health Check
Many of us have not driven as many kilometers this past year as when the world was "normal". Because of this, it may not be evident to you that your vehicle could be developing concerns. Multi...
Blog April 1st, 2021
What is Road Force Balancing?
The machine presses a big roller against the spinning tire's tread. The roller applies 1,200 to 1,400 pounds of pressure to simulate the vehicle's weight. By measuring both the tire and wheel ...
The Value Of A Vehicle Health Check June 15th, 2021
What is Road Force Balancing? April 1st, 2021
How To Get The Most Out Of Your Tires March 4th, 2021
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Jennifer Beattie is the freelance journalist for FD Platinum. With lots of experience of moving and relocating nationally and internationally, Jennifer has personal and professional knowledge of the issues involved. She aims to provide up to date and accurate information on topics of importance to the industry.


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Presentation	Groupe LÉA!	2020-03-05T20:01:47+00:00
LEA! (Lire en Europe Aujourd'hui | Reading in Europe Today) is an international network, created on December 2007, which brings together professorslecturers and/or researchers from Belgium, Hungary, France, Switzerland, Italy, Spain and Portugal thus drawing a true North-South axis of European research.
Directors or members of renowned laboratories and research centres, they are all specialists in French, francophone or comparative literature from the 19th to the 20th century, without excluding the more contemporary; the fields of research on which they work are diverse: novel, short story, theatre, poetry, essay, theory of reading, theory of fiction, poetry of the novel, literary translation… In face of what was called, too hastily, the "decline" of the Human Sciences, reflected throughout Europe through institutional situations, often critical, these researchers who met frequently during other exchange programs or that are currently associated to other projects wished to join forces to contribute to the international spreading of literature and literary studies.
Their common subject is French and Francophone Literature, often overshadowed by a narrow "Franco-French" point of view, from the margins and borders. Far from trying to dilute the reflection on literature and its teaching in the "all cultural" (Communication "Cultural Studies"), the research group LEA! intends to emphasize on theoretical research and continuing education, and is therefore particularly open to young researchers and PhD students interested in these issues.
Since its foundation, LEA! has organized multiple meetings and initiatives, including numerous international symposia, publications and a series of summer schools, the last of which took place in Braga (Portugal) on "Les Études littéraires aujourd'hui? Enjeux et atouts d'une indiscipline" ("Literary Studies today? Issues and strengths of indiscipline") (July 2019), and the next one will be held at the Universitat de València (Spain) on the theme "Mutations", in July 2020 (see Intensive Programs).
LEA – Lire en Europe Aujourd'hui – Lire et écrire des textes littéraires à l'époque des humanités numériques / Reading in Europe today – Reading and Writing Literary Texts in the Age of Digital Humanities
Thanks to the Erasmus+ Strategic Partnership action, the LEA! group has obtained a grant to carry on for three years its project on reading strategies and publishing of literary and critical texts. The dossier was filed by Pázmány Péter Catholic University of Budapest. During the three years of the project development, French, Portuguese, Spanish, Luxembourgish, Belgian and Hungarian researchers from 13 European universities, members of the LEA! group, will try to find out what new methods can be applied to think differently about the reading experience, indispensable to life.


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FOR IMMEDIATE RELEASE CONTACT: Jack Buckley
October 22, 2010 781- 389-2835
Massachusetts Law Enforcement Leaders Praise Coakley's
Record and Vision on Keeping People Safe and Preventing Crime
BOSTON – Citing her twenty-five of experience as a prosecutor, District Attorney, and Attorney General, and her efforts to support law enforcement, protect victims and keep people safe, the Massachusetts Municipal Police Coalition (MMPC) endorsed Martha Coakley today for re-election as Attorney General.
"I'm proud to have the support of the MMPC, but I'm also inspired by their work each and every day to keep our cities and communities safe," said AG Coakley. "As a prosecutor, your first job is to protect the people of the Commonwealth. And this race is about choosing an Attorney General who best stand up for consumers, taxpayers, and families during these difficult economic times. As your Attorney General, I will continue to work with the MMPC and law enforcement leaders from across the state to protect you and your families, and I will never back down."
"As District Attorney and Attorney General, Martha Coakley has been an ally and a friend to law enforcement, because she understands that by working together we can keep our communities safe for our children and our families," said MMPC President Harold MacGilvray. "AG Coakley's 25 years of experience protecting the people of Massachusetts is unmatched and we strongly support her re-election, so she can continue her work supporting victims, protecting our children online and in their neighborhoods, and preventing crime across the state.
To date, Coakley also earned the support of a wide range of law enforcement groups and leaders, including District Attorneys, police officers, and advocates for child safety.
As a federal prosecutor, an Assistant District Attorney, Middlesex District Attorney, and now as Attorney General, Coakley has an unmatched record in this race of protecting our kids and communities. As a prosecutor for the Middlesex DA's Office, Martha has personally and successfully prosecuted dozens of violent criminals in Massachusetts. As Chief of the Middlesex DA's child abuse unit, Martha oversaw the prosecution of hundreds of predators who harmed children.
Martha Coakley is the only candidate in this race who has prioritized victim support and public safety challenges such as cyber crime, senior safety, neighborhood safety, and child protection. Her opponent has remained virtually silent on these critical issues throughout the past two months. Coakley's wide-ranging endorsements today are reflective of her 25-year commitment to making the Commonwealth a safer place and her record of not just prosecuting crime, but working in collaboration with all involved to prevent future tragedies.
As Attorney General, Martha has been a national leader in working to protect people online. As part of her Cyber Crime Initiative, Coakley revolutionized the tools available to prosecutors for fighting crime in the 21st century, ensuring that Massachusetts is on the forefront of public safety challenges. Her office trains local and state law enforcement officers in how to handle cyber crimes, with specialized trainings on topics such as digital evidence, cyber-bullying, and others. She also opened a state of the art computer forensics laboratory that assists with criminal cases from across the Commonwealth.
In 2008, Coakley led a two-year effort with MySpace and Attorneys General across the country to develop a plan to make social networking sites safer for children. She also successfully took on Craigslist by calling on the site to take down its adult services section to better protect victims of human trafficking.
8995 hits since Feb 08, 2011


text:
\section{Introduction}
\pds\ was discovered as a radio-quiet luminous quasar in the course of the Pico dos Dias survey (PDS)
of bright IRAS sources \citep{torres97}.
The optical spectrum of \pds\ features broad emission lines and a redenning-corrected luminosity 30\% higher than that of 3C\,273 \citep{simpson99}.
The high luminosity of \pds\ provides a low limit of $10^9$~M$_\odot$ on the black hole mass, just from the Eddington limit.
Rapid \x\ variability of \pds\ was first noticed with the {\small \it RXTE}\ satellite in 1998 by \citet{reeves00}, who observed the 2 -- 10 keV flux double in 17~ks, which is rather uncommon for such a luminous quasar and indicative of an unusually compact source of a few gravitational radii.

A few years later, \citet{reeves03} reported an ultra high velocity outflow from \pds\ based on blue-shifted Fe K-shell absorption features detected in a 40~ks {\small \it XMM-Newton}\ observation from 2001.
Extremely blue-shifted Fe-K absorption has been reported for other quasars as well
\citep[e.g.,][]{chartas02, chartas03, poundsPG12},
Obviously, for a confirmed detection of an outflow and for conclusive velocity measurements,
it is most desirable to observe as many resolved lines as possible, all shifted by the same velocity.
This is most difficult, since in many objects the absorption is detected primarily from the most highly ionized species of Fe,
whose lines occur at energies where the sensitivity of current detectors drops sharply, and in ionization regimes that preclude absorption by all other species that are too (fully) ionized to produce lines.
The difficulty is then augmented by the rapid spectral variability of these outflows \citep{kaspi05, chartas07, reeves08}, which imposes fundamental limits on the signal-to-noise-ratio (S/N) of spectra and deems data stacking from separate observations almost useless.
All these have raised questions regarding the statistical robustness of some, but probably not all, of the blue-shifted absorption detections \citep{vaughan08}.
The only way to substantiate and further study these high velocity outflows is with long exposures and  high S/N spectra, such as the present one.

\pds\ stands out as one of the least controversial ultra high velocity outflows.
Not only does it have multiple Fe-K absorption detections over the years \citep{reeves00, reeves03, reeves09}, but a 2001 {\small \it XMM-Newton}\ observation revealed an absorption feature in the soft \x\ band that was measured at high-resolution with the Reflection Grating Spectrometers ({\small RGS}).
Indeed, the {\small RGS}\ spectrum shows a deep and broad absorption trough between 13--14~\AA\ (in the observed frame), interpreted by \citet{reeves03} as due to a $\sim$50,000~\kms\ outflow that also produces the Fe-K absorption edge.
Blue-shifted Ly\,$\alpha$ absorption indicates an appreciably slower outflow moving at 14,000 -- 24,000 \kms\ \citep[][]{obrien05}.
Despite its moderate redshift of $z$ = 0.184, \pds\ is also the brightest among the targets suspected of harboring an ultra high velocity outflow.
With all this in mind, we obtained a deep {\small \it XMM-Newton}\ exposure of \pds, which is reported in this paper.
{\small \it XMM-Newton}\ has the largest effective area of all current \x\ telescopes and thus provides the best chance to observe several absorption lines from the same outflow component with the gratings.

In the meantime, a {\small \it Suzaku}\ observation of \pds\ provided another high-quality (though low-resolution) spectrum of \pds\ in which Fe-K line shifts of 100,000 \kms\ were detected at high S/N, but with no obvious soft \x\ line absorption \citep{reeves09}. This adds to the mounting evidence of blue-shifted absorption detected in \pds\ above 8~keV.  An exciting discovery in the {\small \it Suzaku}\ observation is the significant emission at high energies above 15~keV, much in excess of the extrapolated soft \x\ spectrum.
This is yet another manifestation of the unique spectral behavior exhibited by this intriguing quasar.
In the present paper, after analyzing the 2007 observations and studying the short term \x\ variability within those two {\small \it XMM-Newton}\ orbits  in Section~\ref{sec:xmm07}, in Section~\ref{sec:partabs} we also study the spectral variability of \pds\ between different epochs, and on time scales of months and years, over the past decade.

\section{Observations}
\label{datareduction}

\subsection{Data Reduction and Light Curves}

In Table~\ref{obs_log} we list the log of the 2007 {\small \it XMM-Newton}\ observations of \pds\ as well as the earlier {\small \it XMM-Newton}\ observation from 2001, and then the other observations of \pds\ that are used later in this paper.
{\small \it XMM-Newton}\ data were reduced using the Science Analysis Software (SAS - ver. 7.1.0) in the standard processing chains as described in the ABC Guide to {\small \it XMM-Newton}\ Data Analysis\footnote{See http://heasarc.gsfc.nasa.gov/docs/xmm/abc},
and using the most updated calibration files for 2009, June 15.
Both single and double events were retained and no pile up was detected.
1.5~ks were excluded from the orbit-1421 data set due to high background.

The light curve of the source during orbits 1421 and 1422 is shown in Fig.~\ref{fig:lc}.
The source flux diminishes gradually during the second orbit to approximately half its initial flux level.
The typical time for variability in Fig.~\ref{fig:lc} is $\sim$30\,ks,
similar to that reported by \citet{reeves02}, and which
corresponds to the light crossing time of only a few gravitational radii.
It should be noted that despite the significant \x\ variability of \pds, it is rather steady in longer wavebands.
The optical monitor (OM) on board {\small \it XMM-Newton}\ recorded a flux range of (2.4 -- 2.5) $\times 10^{-15}$ erg\,s$^{-1}$\,cm$^{-2}$\ (1.10 -- 1.14 cts\,s$^{-1}$ during orbit 1421) with the UVM2 filter around 2300~\AA\  and a range of only (5.75 -- 5.85) $\times 10^{-15}$ erg\,s$^{-1}$\,cm$^{-2}$\ (12.1 -- 12.3 cts\,s$^{-1}$  during orbit 1422) with the UVW1 filter around 2900~\AA.
These can be further compared with the archival HST/STIS measured flux of  3 $\times 10^{-15}$ erg\,s$^{-1}$\,cm$^{-2}$\  at 2300~\AA\ and 9.5 $\times 10^{-15}$ erg\,s$^{-1}$\,cm$^{-2}$\  at 2900~\AA\ on 2000, May 14.
All fluxes are quoted before correcting for reddening.
Optical monitoring in the V band carried out at the Wise Observatory every two
weeks over half a year reveals an increase in flux from 2007 April to
July of only 0.05 mag, and then a decrease in flux from 2007 July to October
of 0.07 mag.
Thus, while the X-ray flux varies by a few tens of percent
over a period of a day, the {\small UV}\ flux is constant to within a few percent.
At much longer time scales, perhaps even years but not well monitored,
the {\small UV}\ flux can also vary by a factor of two.
The optical flux varies by only a few percent over several months.
This is not unusual, as quasar monitoring often shows an increase of variability with frequency
from optical, through {\small UV}, and up to the \x\ band \citep{edelson96}.

\subsection{Background}
\label{bg}

In order to obtain the \x\ spectra, we extracted the source photons from the {\small EPIC~PN}\ and {\small MOS}\ cameras in a circular region of radius 40\arcsec\ and grouped the data to bins with minimum 25 counts per bin.
We use the standard SAS background files for each observation, where the background spectrum is extracted from an annulus region centered around the source of 1\arcmin ~to 3\arcmin, from which 1\arcmin\ circular regions around field point sources are excluded.
The background for {\small EPIC~PN}\ requires special caution as it can have strong instrumental, narrow emission lines at energies around 1.5 and 8 keV, which could introduce by subtraction artificial absorption lines.
The background during the 2007 observations was relatively high, but we verified that the background spectra we use have no such lines.

We measured the background in various off-source locations on the {\small EPIC~PN}\ and {\small MOS}\ CCDs.
A sample background spectrum is shown in Fig.~\ref{fig:bg}.
Indeed, instrumental emission lines appear on the detector with varying strengths
as has been documented in the {\small \it XMM-Newton}\ Users'
Handbook\footnote{http://heasarc.gsfc.nasa.gov/docs/xmm/uhb/node35.html}.
\citet{freyberg04} investigated the intrinsic instrument background in the {\small EPIC}\
detectors and found that it is composed of a continuum and X-ray fluorescence lines,
most prominent are those at 1.5, 7.7, 8.0, 8.6, and 17.4 keV, which are due to K$\alpha$
line emission of Al, Ni, Cu, Zn, and Mo, respectively.
The lines show strong spatial inhomogeneities
correlated with the structures of the electronics board mounted below the {\small EPIC~PN}\ CCDs.
\citet{freyberg04} also found that the very central region of the camera where typically the primary source is located is free of this instrumental background.
Therefore, our use of line free background spectra is justified.

We also examined the background in the archival {\small \it XMM-Newton}\ 2001 observation.
For this observation as well, we use the standard 1\arcmin ~to 3\arcmin\ annulus.
The background in the 2001 observation is much lower and its fluorescence lines
much less prominent.
More precisely, at the edge of the CCD the fluorescence lines are strong,
but they get much weaker close to the center of the CCD, as expected \citep{freyberg04}.
Thus, the spectral turnover detected around 8 keV in the 2001 spectrum of \pds\ \citep{reeves03} is
secure and not significantly influenced by the background.

\section{2007 {\small \it XMM-Newton}\ Campaign}
\label{sec:xmm07}

The September 2007 {\small \it XMM-Newton}\ observations provide the highest S/N spectra of \pds\ to date.
{\small EPIC~PN} , for example, collected an estimated 437,600 source photons, compared to 121,700 photons during the 2001 observation.
The spectra of both {\small EPIC}\ cameras and the {\small RGS}\ are of sufficiently high statistical quality to be confronted with a variety of models.
Below 0.4 keV, we find discrepancies of 20\%\ between the {\small EPIC~PN}\ and {\small MOS}\ data with respect to a simple power-law.
Hence, the present modeling is carried out in the 0.4--12.0~keV range and highlights mostly the more sensitive {\small EPIC~PN}.
These spectra are presented separately for the {\small \it XMM-Newton}\ orbits 1421 and 1422 in Fig.~\ref{xmm07}, along with fits to increasingly complex models.
Although the separation of the data into the two {\small \it XMM-Newton}\ orbits is arbitrary,
it provides an insight into the short-term variability and a reality check for persisting spectral features.
It is noted that the {\small EPIC~PN} -fitted models of each orbit also fit the {\small MOS}\ spectra very well.
For presentation purposes alone, we have omitted the {\small MOS}\ data from the plots.

We first fit the spectra with a simple power law absorbed by the nominal neutral H Galactic column density of $N_H = 2.0 \times 10^{21}$~cm$^{-2}$, using the absorption model of \citet{tbabs}.
We find that the photon slope $\Gamma$ slightly increases by 0.05 between the two orbits.
This model alone is clearly inadequate, as seen by the large residuals plotted in the top panel of Fig.~\ref{xmm07}, and since it yields $\chi ^2$/d.o.f = 1.9.
The residuals below 1~keV suggest the neutral column is underestimated.
Indeed, the best-fit neutral column density is $N_H = (2.67 \pm 0.03) \times 10^{21}$~cm$^{-2}$, which considerably improves the fit to $\chi ^2$/d.o.f = 1.19 (middle panel of Fig.~\ref{xmm07}).
Separate fits to the {\small RGS}\ and {\small MOS}\ spectra yield respective column densities of $(2.64 \pm 0.10) \times 10^{21}$~cm$^{-2}$ and $(2.65 \pm 0.05) \times 10^{21}$~cm$^{-2}$, all consistent and robustly above the Galactic column.
The redshift of \pds\ ($z = 0.184$) allows us to test whether the excess column occurs in the quasar, by invoking a redshifted absorption component in the model.
However, the fit decisively ascribes the entire neutral column to the $z = 0$ component and no column to the redshifted one.
Moreover, if the redshift of the additional component is left to float, the fit requires that it converges to $z = 0$.
The agreement between {\small EPIC~PN} , {\small MOS} , and {\small RGS}\ imply that detector contamination can not be the reason for the excess absorption \citep[see also][]{kirsch05}.
We tested whether perhaps a partially covering absorber can explain the excess low-energy absorption.
However, the best fit model of a partial covering neutral absorber yields a covering fraction of 100\%
(and with no improvement to $\chi ^2$/d.o.f = 1.19).
There is also no indication of an ionized absorber that could be responsible for the excess absorption, as no absorption lines are detected anywhere in the spectra.
Indeed, the best fit for a partial covering ionized absorber yields a column density that tends to zero, and again no improvement to $\chi ^2$/d.o.f = 1.19.

To make a long story short, the data clearly indicate excess neutral absorption that is consistent with $z~= 0$. Although in principle it is possible that by coincidence this absorption is due to gas in \pds\ that happens to be outflowing by exactly the cosmological recession velocity of the quasar, we reject this notion as highly unlikely.
Moreover, since all indications point to this absorber being neutral, we do not associate it with the highly ionized outflows observed in \pds.
Similar variable Galactic absorption has been detected towards  NRAO 140, where it could be explained by motion in the Perseus molecular cloud complex \citep{turner95}.
Does the moderately low Galactic latitude of \pds\ of +11$^\circ$ suggest a similar explanation in the present case?
We searched for any molecular clouds towards \pds, both in the IRAS archive, and in the Columbia CO survey \citep{dame87}, but found none.
The origin, therefore, of the excess neutral absorption and its discrepancy with previous measurements remains somewhat unclear.

In the middle panel of Fig.~\ref{xmm07}, we show the spectral residuals that remain after incorporating the higher column density in the model.
It can be seen that these residuals are fairly similar in both orbits (but keep in mind the slightly different power law slopes).
The residuals below 1~keV could be due to the incomplete absorption model around the O-K ($\sim 0.53$~keV) and Fe-L ($\sim 0.71$~keV) photoelectric edges.
At high energies, there is excess emission around the Fe-K region between 5 and 7 keV in the observed frame.
Note that much of this emission is blueshifted with respect to the quasar frame, given that the 6.4 -- 7.0~keV range of Fe-K lines corresponds in the observed frame (Fig.~\ref{xmm07}) to the 5.4 -- 5.9~keV energy range.
The Fe-K excess emission and its high statistical significance is further demonstrated in the $\chi ^2$ residuals plotted in Fig.~\ref{FeK}.
The second data set (orbit 1422) has a narrow component, but both data sets feature large broad residuals resembling the electron-scattered blue wings typical of ionized (Compton) reflection.
Also important is the over all curvature of the model between 1 and 5 keV, where no narrow features occur, that is not properly reproduced by an absorbed power law.
Together with the Fe-K residuals this strongly suggests a reflection spectral component.
Indeed, adding a constant density reflection component \citep[{\it reflion}, by][]{ross05} notably and significantly improves the agreement of the model with the data ($\Delta \chi ^2 = 313$, and $\chi ^2$/d.o.f = 1.05).
The broad-band spectral curvature between 1 and 5 keV is also much improved when reflection is included in the model, as can be seen by comparing the middle and bottom panels of Fig.~\ref{xmm07}.
The small remaining residuals are of order of 10~-- 15~\%.
The best-fit parameter values for the two combined orbits are given in Table~\ref{tab:fit07}.
When fitting the two data sets separately, we find that the reflection component fits the second data set (orbit 1422) particularly well, yielding $\chi ^2$/d.o.f = 0.99. The fit to the first spectrum (orbit 1421) is somewhat poorer with $\chi ^2$/d.o.f = 1.10.  Models fitted separately to each spectrum yield parameters that are similar to those of Table~\ref{tab:fit07} ($\log \xi \approx 4, A_{\mathrm Fe} \approx 3, z \approx 0.1$), but are not as  tightly constrained.

We tested alternative models to reflection, including a plain Gaussian emission line and a gravitationally distorted emission line.
Both give unphysical results as could have been expected from the spectral shape of the residuals and the combined narrow and broad nature of the residuals in the middle panel of Fig.~\ref{xmm07}.
A Gaussian fit forces an enormously broad feature with $\sigma$~= 3~keV, and centered at an unreasonably low energy of $\approx 4$~keV in the quasar frame, essentially mimicking the underlying broad reflection continuum.
A relativistically distorted line profile \citep{laor91} also yields unreasonable physical parameters, such as a disk inclination of almost 90$^\circ$ and an emissivity that {\it increases} with radius.
Moreover, partial covering neutral, and partial covering ionized absorption models were also tried in place of reflection, but could not eliminate the residuals observed in the middle panel of Fig.~\ref{xmm07}.
In summary, we prefer the reflection model, which is most appropriate for describing both the broad-band and the Fe-K spectrum of \pds\ during the 2007 {\small \it XMM-Newton}\ observations.

The fit of the reflection model to the combined 2007 spectrum constrains the frame of reference of the reflection component rather tightly.
This comes from the position of the reflected Fe line (for $\log \xi \approx 4$ primarily H-like at 6.97~keV) and even more from the electron-scattered blue wings of the line that give it a slightly broadened and skewed profile \cite[see, e.g., Fig.~3 in][and also Fig.~\ref{abs_models} below]{ross05}.
Interestingly, the best-fit redshift for the reflection model is indicative of a frame of reference that is distinct from both the quasar and the observer, namely $z = 0.12 \pm 0.02$ to be compared with $z = 0.184$ for \pds.
Fixing the reflection redshift to that of the quasar and refitting results in an inferior fit ($\Delta \chi ^2 = 28$ resulting in $\chi ^2$/d.o.f. = 1.07).
The intermediate reference frame can be understood as reflection off of fast moving gas,
perhaps the outflows detected in previous observations?
Since both the frame of reference and the ionization state of the reflecting medium bear on the position of its Fe-K line, it is important to investigate the connection between the two in the fit.
In Fig.~\ref{contours}, we plot the combined statistical confidence contours for the redshift and the ionization parameter.
The plot demonstrates that the kinematical shift (i.e., outflow) of the reflector is statistically robust ($> 3\sigma$) against the ionization uncertainties within the framework of the present model.
However, this result is model dependent and a realistic outflow is surely more complicated than the slab reflection used here.
The regime of ionization parameter beyond $\xi~=$ 10,000 (cgs units) is inaccessible with the current reflection models, and therefore is not plotted in Fig.~\ref{contours}.
Moreover, the constraints on each {\small \it XMM-Newton}\ data set when fitted separately are insufficient to produce similar contour plots, only the combined fit is well constrained.
On the other hand, much higher ionization ($\xi~>$ 10,000 in cgs units) can not shift the line position to beyond its current H-like position, which suggests that even higher ionization would perhaps not invalidate the outflowing nature of the reflector.
There is also no obvious indication by extrapolation of Fig.~\ref{contours} that higher ionization compromises the redshift.
The putative radial velocity of the reflector, which would be moving more or less parallel to
but outside the line of sight is
$v_\mathrm{out} / c \approx (0.12 \pm 0.02) - 0.184 = -0.06 \pm 0.02$,
or $v_\mathrm{out} = -18,000~\pm 6,000$~\kms.
In the next section, we show that the moving reflection component may be a persistent feature of the otherwise variable \x\ source in \pds.

Furthermore, if the observed reflection component is due to reflection of the observed primary power law,
it is possible to estimate the solid angle occupied by the reflector as viewed from the primary source.
In a simplified geometry with perfect reflection (i.e., no flux losses on the reflector), and neglecting time lag, the flux ratio of the reflection component to the primary power law gives a rough idea of this fractional sky coverage $\Omega _\mathrm{refl}/ 2\pi$.
The no-losses approximation is reasonable for electron reflection in a nearly fully ionized reflector.
The \citet{ross05} model assumes uniform illumination of the reflector and a plane parallel geometry.
It computes the reflection integrated over all angles from 1~eV to 1~MeV by a power law source ranging from 1~eV to 0.3~MeV.
For the present models, the flux ratio in the observed region from 0.4 -- 12.0 keV gives essentially the same result as that in the full range.
For the best fit model, this flux ratio implies $\Omega _\mathrm{refl}/ 2\pi \approx 0.2$.
The best-fit reflected flux in the present models happens to be similar in both orbits, despite the decrease by approximately 30\% of the mean primary power law flux.
This indicates the reflector is likely extended from the source.

Given the multi-component nature of the \pds\ \x\ spectrum, and given the variability of shifted emission and absorption on short and long time scales, as well as the low Galactic latitude (+11$^\circ$) of \pds , it is worthwhile to examine the viability of a previously unknown Galactic source along the line of sight.
An \x\ binary (XRB) could be the primary candidate for such a source.
In order to test such a conjecture, we inspected the \x\ {\it Chandra}\ image, the {\small UV}\ {\small \it XMM-Newton}\ optical monitor (OM) image, and the 2MASS K-band image of \pds.
They are all perfectly consistent with point sources and are co-aligned to within a fraction of an arcsecond.
By extrapolating the $\log N - \log S$ distribution of \citet{grimm02} for galactic XRBs down to a flux, say, of $f = 10^{-12}$ erg\,s$^{-1}$\,cm$^{-2}$\ \citep[about 10\% of the current flux of \pds, but two orders of magnitude fainter than the completeness limit of][]{grimm02}, one can use the expression $N(>S) = 72(f/3.2\times 10^{-10}$ erg\,s$^{-1}$\,cm$^{-2}$ )$^{-0.41}$ to estimate the number of XRBs in the sky that are brighter than 10$^{-12}$ erg\,s$^{-1}$\,cm$^{-2}$\ to be not more than 800.
Consequently, the probability for a random XRB within the solid angle of 0.5\arcsec $^2$ is $< 4\times 10^{-10}$; negligibly small.  In other words, it seems unlikely that a foreground XRB is present along the line of sight to \pds.

In Section~\ref{sec:partabs}, we explore partial covering models by outflows as a way to explain on an equal footing the entire slew of \x\ spectra obtained for \pds\ over the past decade.
In the 2007 {\small EPIC~PN}\ spectra shown in Fig.~\ref{xmm07} there is no obvious absorption by an outflow, and thus the absorption models actually do not improve the fit.
The reflection component, on the other hand, seems to persist in all epochs.

\subsection{Outflow?}
We searched the present 2007 data set for the fast outflows detected by \citet{reeves03, reeves09}.
The high-energy region of the {\small EPIC~PN}\ spectrum during orbit 1421 is shown in Fig.~\ref{FeK}.
No sign of absorption can be detected whatsoever;
Neither the lines that appear in the {\small \it Suzaku}\ spectrum at 7.67~keV and 8.13~keV \citep{reeves09}, nor the edge that appeared in the 2001 {\small \it XMM-Newton}\ observation \citep{reeves03} are seen in this data set.
We further inspected the {\small RGS}\ spectra from both {\small \it XMM-Newton}\ orbits.
Fig.~\ref{RGSpanels07} presents the ratio of the {\small RGS}\ spectra to the model used above to fit the {\small EPIC~PN}\ spectra, with no adjustments whatsoever.
Since this model includes no discrete spectroscopic features (except perhaps the neutral O absorption at $\approx$ 23.5~\AA), we would expect absorption (or emission) lines or edges due to the outflow to show up in the {\small RGS}\ data.
We show in Fig.~\ref{RGSpanels07} each {\small RGS}\ (1 and 2) and the data of each orbit separately in an attempt to identify outstanding features.
The statistics of the data presented is rather high, ranging from over 5,000 to over 10,000 source photons in each panel, which are distributed over $\approx$~170 bins.
In fact, this is the best high-resolution \x\ spectrum of \pds\ to date.
A closer look into the 13--20~\AA\ spectral region, where the {\small RGS}\ is most sensitive, is presented in Fig.~\ref{RGSzoom07}.
We are unable to identify any recurring lines that appear in all of the panels of Figs.~\ref{RGSpanels07} or \ref{RGSzoom07}.
At the very least, we would expect genuine absorption lines to be present in both RGSs during a single observation (panels 1 and 2, or 3 and 4), but we find none.
We conclude that there is no unambiguous sign in September 2007 of the outflows detected in the two previous observations.
The intermittent nature of the outflow has immediate implications on the overall AGN energy budget as affected by such flows.

\section{Spectral Variability}
\label{sec:partabs}

The appearance and disappearance of the outflow in \pds\ within several months is only one aspect of the full range of changes taking place in this intriguing quasar.
Since it was discovered, \pds\ was observed by almost all available \x\ telescopes.
Therefore, one can expect to obtain a more comprehensive picture of this source by studying its \x\ spectral history.
In addition to the current data sets from the two {\small \it XMM-Newton}\ orbits in 2007,
there are five archival \x\ observations of \pds.
These are available from {\small \it XMM-Newton}\ (February 2001), {\small \it Suzaku}\ (February 2007), {\it Chandra}\ (May 2003), {\small \it ASCA}\ (March 1998), and {\small \it RXTE}\ (February-March 2001).
With the exception of {\it Chandra}, all observations were reported in the literature
 \citep{reeves00, reeves03, reeves09}.
For the details about these data and how they were reduced we refer the readers to those references.
The {\it Chandra}\ {\small HETGS}\ observation was not published because it caught \pds\ in a very low state.
The data are reduced here using CIAO version 3.2.1 and CALDB 3.0.1 and the standard CIAO threads.
Spectral fits were carried out simultaneously for both {\small HETGS}\ instruments (MEG and HEG),
although we show only the MEG spectra.
In Fig.~\ref{fullcomp}, we plot the ratio of the different \pds\ spectra to a simple Galactically absorbed ($N_H = 2 \times 10^{21}$~\cmii) power-law with photon index $\Gamma = 2$.
From the 2007 {\small \it XMM-Newton}\ campaign, only the spectrum of orbit 1421 is presented, to minimize crowding of the plot.
The total flux variability is of the order of a factor of 2--3.
This may not be expected from a quasar as bright as \pds\ ($L_X \approx 10^{47}$~erg~s$^{-1}$).
However, \pds\ has already been observed varying by a factor of a few over less than a day \citep{reeves00}.

From Fig.~~\ref{fullcomp}, it can be seen that spectral structure below 1~keV varies both overall and in its narrow features.
The Fe-K region beyond 5~keV also changes drastically.
What appears as an absorption edge, and can be interpreted as an outflow, varies both in position and in depth.
The significance of emission features, possibly identified as due to reflection, changes as well.
Between 1~keV and 5~keV, the spectral curvature changes in what seems to be an intricate combination of emission and absorption variability.
This observed complexity can not be characterized by a single spectral component or one obvious spectral parameter, such as power-law slope, Fe-K line flux, or absorbing column density.
What on the face of it seem to be common features in several spectra,
such as an Fe-K absorption edge (or emission line?) beyond 6~keV,
or an Fe-L emission hump below 1~keV,
upon closer inspection in fact appear to occur at slightly different energies in each spectrum.

In the next section, we attempt to use one possible type of models to fit all of the spectra of \pds.
For this exercise we fit separately six epochs with high quality CCD data at an energy resolution of $\Delta E \approx 100$~eV, or better, namely those of {\small EPIC~PN}\ (two {\small \it XMM-Newton}\ orbits in September 2007), {\small EPIC~PN}\ (2001), {\small \it Suzaku}\ XIS 0 \& 3 (February 2007), {\it Chandra}\ {\small HETGS}\  (2003, MEG \& HEG) rebinned to CCD resolution due to low S/N, and {\small \it ASCA}\ SIS (1998).
We leave out the {\small \it RXTE}\ spectrum due to its lower resolution.
Data from {\small MOS}\ on {\small \it XMM-Newton}\ and XIS~1 on {\small \it Suzaku}\ are less sensitive at high energies, but their data are consistent with those of {\small EPIC~PN}\ and XIS 0 \& 3, respectively \citep[see][]{reeves03, reeves09}.
The six data sets used here are listed in Table~\ref{obs_log}. The modeling strategy is described in the next section.

\subsection{Partial Covering Approach}
\label{sec:pc}
For the model, we invoke a simple continuum power law source, partially covered by a (possibly ionized) absorber and absorbed locally in our Galaxy.
For the absorbing outflow, the analytical {\it warmabs} models version 2.1ln8 of {\small \it XSTAR}\ \citep{xstar01} available in {\small \it Xspec}\  are used \footnote{http://heasarc.gsfc.nasa.gov/docs/xanadu/xspec/models/xstar.html}.
A reflection component is also included as in Section~\ref{sec:xmm07}, to account simultaneously for Fe-K lines and for the soft excess that is observed in some data sets and apparently varies in its discrete features (Fig.~\ref{fullcomp}).
In {\small \it Xspec}\ code, the model used is {\it TBabs} ({\it zpowerlw + zpowerlw * warmabs * warmabs + reflion}).
That partial covering of the central source can provide useful insights into the AGN geometry was realized by \citet{reichert86}.
These types of models provide a wide range of broad band spectral curvature that may (or may not) be able to produce the vastly different spectra seen in Fig.~\ref{fullcomp}.
The model discussed above for the 2007 {\small \it XMM-Newton}\ spectra (Section~\ref{sec:xmm07}) where no absorption is detected qualifies as the degenerate extreme case of zero coverage of the source.
Realistic partial covering models also include narrow absorption lines, which impose additional constraints complementary to the broad-band curvature of the spectrum.
However, when $\chi ^2$ minimization techniques are used to select models, as in the present work,
the continuum statistics overwhelms that of the discrete features.
Thus, the narrow features are much harder to constrain with the current CCD spectra.
Similar models of partial covering by an ionized outflow have been tried with relative success by \citet{reeves03} for the 2001 observation of \pds, and recently by \citet{miller08} for MCG\,-6-30-15.

The modest goal of this section is to test the conjecture that perhaps it is the varying fractional coverage of the source by the outflow that drives the spectral variability, and whether these models can provide an acceptable overall explanation to {\it all} of the six spectra of \pds.
This type of partial coverage models is complex and invokes by far more parameters than can be constrained by the data.
Consequently, it is beneficial to fix a-priori as many parameters as possible.
The illuminating spectrum to be absorbed and reflected is the aforementioned power law with its slope fixed to $\Gamma = 2.25$, which is the best fit value for the high S/N and relatively featureless spectra obtained with {\small EPIC~PN}\ (orbit 1422) and with  {\small \it Suzaku}.
Two ionization components are included for the absorber.
These components represent high and low ionization in an absorber that more realistically could have a continuous distribution of charge states \citep{steenbrugge03, behar09}, and are therefore not well constrained by low-resolution data.
The fractional coverage of the power law source by the outflow is a fitted parameter.
The outflow velocity is fitted in each spectrum and is found to somewhat vary from one observation to the other. The velocity broadening is fixed at $v_\mathrm{turb}$ = 2,500~\kms, which fits well the only grating measurement of absorption lines in \pds\ (see Section~\ref{sec:rgs01} below) and is consistent with the width of the absorption lines in the {\small \it Suzaku}\ spectrum \citep{reeves09}.

Since the reflection component in the 2007 {\small \it XMM-Newton}\ spectra appeared to be moving (Section~\ref{sec:xmm07}) and inconsistent with the rest frame of \pds,
it may be moving with the absorbing medium.
Consequently, we tie the outflow velocities of the reflection and absorption components,
which would be a good approximation as long as the opening angle of the putative reflecting outflow is not too large.
Abundances are set to their solar values, except for the Fe abundance of the reflector that is set at three times solar as required by the fits in Section~\ref{sec:xmm07}.
No independent Fe-K absorption or emission feature beyond the outflow and reflection features is added.
Also for simplicity, no relativistic blurring is invoked, since it tends to
make the models even more degenerate than they already are.
Despite all of these impositions on the model, it is still fairly degenerate and the fit can not reliably constrain all of its free parameters.
To that end, the {\small \it Suzaku}\ spectrum can be singled out with its detected absorption lines from two kinematic components and the ionization parameter that can be more accurately determined \citep{reeves09}.
Consequently, in our model for the {\small \it Suzaku}\ spectrum, the absorber ($v/c \approx -0.3$) and reflector ($v/c \approx -0.12$) are allowed to have different velocities.

\subsection{Fit Results}
\label{fit_results}

Using the partial covering model with its restricted parameters as described above,
we fitted the six available spectra.
The results are presented in Fig.~\ref{abs_models} in the form of unfolded spectra.
It is worth warning that unfolded spectra should not be used to confirm spectral features in the data, but rather to present what a best-fit model spectrum would look like assuming it well represents the source spectrum.
In each panel of Fig.~\ref{abs_models}, the different model components are plotted, namely the absorbed power law that turns over above 2~keV, the unabsorbed power law that turns over only below 1~keV due to Galactic  absorption, and the reflection component.
The relative contributions of the absorbed and unabsorbed components, i.e. the partial covering, varies dramatically between epochs.
The absorbed component is very weak in the 2007 {\small \it XMM-Newton}\ observations (top panels of Fig.~\ref{abs_models}), as the fit provides only upper limits to its presence and indicates very low covering fraction ($<20\%$), if any.
Such an absorber would be consistent with the highly absorbed hard \x\ component detected with {\small \it Suzaku}\ by \citet{reeves09}, but we can not conclusively confirm its presence in the 2007 {\small \it XMM-Newton}\ spectra.
The reflection contribution to the total flux is generally small, but persistent in all epochs, and its
emission below 1~keV is required to produce the soft excess observed in some of the spectra as well as the Fe-K line emission and the spectral drop off above 5~keV.
It can be seen from Fig.~\ref{abs_models} that the models provide reasonable representations of the wide variety of spectra observed from \pds.
Despite the several fixed parameters and most notably the power law slope,
by varying the column densities and the fractional covering by the outflow,
the quality of the fits is reasonable with $\chi ^2$ / d.o.f $\approx$ 1.0 -- 1.3, although not always statistically acceptable.
We believe the imperfect fits are not necessarily due to the inadequacy of partial covering for describing \pds\ at all epochs.
More likely, it is the shortcomings of the models and their incomplete detail.
In some cases, calibration issues can also affect the fits.
For example, ignoring the instrumental Si edge region of the {\small \it Suzaku}\ spectrum between 1.75 and 1.9~keV dramatically improves $\chi ^2$ / d.o.f from 1.30 to 1.20.

The best-fit model parameters for the six spectra are summarized in Table~\ref{table:fit}.
In light of the excessive local column density found in the 2007 {\small \it XMM-Newton}\ observations,
the absorption in the model is allowed to exceed the nominal Galactic value of $N_H = 2 \times 10^{21}$~\cmii.
However, the slightly higher local column density detected in the 2007 {\small \it XMM-Newton}\ spectra ($N_H = 2.7 \times 10^{21}$~\cmii , see Section~\ref{sec:xmm07}) is not required in other epochs, except perhaps in the lower-quality {\small \it ASCA}\ spectrum where it is not as well constrained.
As discussed in Section~\ref{sec:xmm07}, this excess must be in our own galaxy (or at $z = 0$),
but why it varies remains unclear.
In the 2007 {\small \it XMM-Newton}\ observations (top two panels in Fig.~\ref{abs_models}), the unabsorbed component dominates (i.e., low covering fraction) and the outflow, if at all present, covers not more than 20\% of the source;
In the {\small \it Suzaku}, {\small \it ASCA}, and {\it Chandra}\ spectra, it is the absorbed continuum that dominates (i.e., almost full coverage), while the model for the 2001 {\small \it XMM-Newton}\ observation suggests an intermediate case in which about half of the source is covered by the absorber.
Thus, the variation of the partial covering fraction can explain much of the spectral variability observed in \pds.
This would place the absorber at a distance from the source that is comparable to the source size.
Variable partial covering, however, can also be due to many small sources, e.g., an assortment of magnetic flares above an accretion disk, some of which are absorbed and some of which are not.
The size of the patchy absorber then would be of the accretion disk scale.

Apparently, the column density in the absorption components also varies dramatically between epochs.
A column of a few times 10$^{22}$\,\cmii\ or higher can account for the spectral curvature between 2~-- 5~keV, which is observed in the 2001 {\small \it XMM-Newton}, the {\small \it ASCA}, and the {\it Chandra}\ spectra.
The {\small \it Suzaku}\ spectrum requires only the two high-ionization ($\log \xi > 3.5$) absorbers that produce the blueshifted Fe-K absorption lines \citep{reeves09} and that cover most of the source.
In the 2007 {\small \it XMM-Newton}\ spectra, the alleged absorber does not significantly affect the spectrum up to 12~keV.
Indeed, the fits with absorption do not represent an improvement over those without absorption presented in Section~\ref{sec:xmm07}, despite the high column densities (but low covering fraction).
The absorption model in the 2001 {\small \it XMM-Newton}\ observation requires (at least) two components,
and it needs to describe the absorption detected in the (simultaneous) {\small RGS}\ spectrum of the same observation.
The most conspicuous absorption feature in that {\small RGS}\ spectrum occurs at approximately 0.9~keV and can be discerned with the CCDs.
Such deep absorption lines require an absorber that essentially fully covers the source.
On the other hand, partial covering is required to produce the observed broad-band curvature of the spectrum.
This result was already reported by \citet{reeves03}.
Hence, the model proposed here for the 2001 {\small \it XMM-Newton}\ observation, which is shown in Fig.~\ref{abs_models}, has a high-ionization absorber fully covering the source and a low ionization component only partially covering it ($\approx 50\%$), both with columns of a few times 10$^{22}$\,\cmii.
An additional component may be needed to fully account for the deep and blueshifted Fe-K edge observed at 7~-- 8~keV \citep[see Fig.~\ref{abs_models} and][]{reeves03}.

The reflection component is consistently present in all epochs.
Its relatively moderate flux indicates the reflector only partially intercepts the \x s from the primary power law source.
In fact, the models for all six epochs indicate it reflects about 20\% of the primary source (see also Section~\ref{sec:xmm07}).
This result is generally consistent with reflection off a moderately collimated outflow.
However, if the outflow is patchy as suggested by the varying partial covering,
the outflow segments can in fact be spread over a broader solid angle.
In the 2007 {\small \it XMM-Newton}\ observations, the reflecting matter appears highly ionized ($\log \xi$ up to 4) and thus does not produce the soft \x\ emission that appears in all of the other epochs where it is approximately in the $2 \mathrel{\rlap{\lower4pt\hbox{$\sim$}  \log \xi \mathrel{\rlap{\lower4pt\hbox{$\sim$} 3$ range.
The reflection models tend to systematically prefer a super-solar Fe abundance,
although the exact value is poorly constrained.
We deem such a high Fe abundance to be unphysical, and ascribe it mostly to the shortcomings of the model, rather than to an actual abundance effect.
Since in any case, without multiple identifiable narrow features it is impossible to expect a reliable assessment of abundances,
we fix the Fe abundance at three times solar (Section~\ref{sec:xmm07}).
The outflow velocities of the absorber/reflector are mostly constrained by the soft \x\ emission lines in the reflection component, which yields effective redshifts in most cases of $z = 0.10 - 0.14$.
If associated with an outflow in the reference frame of \pds\ ($z = 0.184$),
these redshifts translate into outflow velocities of $v_\mathrm{out}/c \approx$ --0.04 to --0.08.
Two exceptions to this velocity range are noted.
The first is the {\small \it Suzaku}\ spectrum in which the narrow absorption lines require a much faster outflow of $v_\mathrm{out}/c =$~--0.26 and --0.31 as reported by \citet{reeves09}.
The second exception is the 2001 {\small \it XMM-Newton}\ observation that has a deep blueshifted edge-like feature at approximately 8~keV.
When ascribed to the outflow, this edge implies $v_\mathrm{out}/c \approx$~--0.19 \citep{reeves03}.

Although the reflection component of the model does produce the observed flux below 1~keV, it does not always match all of the spectral details very well.
Consequently, at least formally, the fits are not always statistically acceptable.
Indeed, invoking a partial covering absorber inserts additional uncertainty, as the fit is only partially sensitive to adding continuum and absorbing it.
Nonetheless, we suspect the deficient fits are likely due to shortcomings of the detailed models we use,
and do not necessarily invalidate the relevance of partial covering or reflection.
For example, even moderate broadening of discrete reflection features, due to velocity or to scattering, would make them less prominent.
Also, incomplete atomic data, the constant-density approximation, and the simplistic geometry used in the reflection model certainly affect the goodness of the fit.
Discrete features detected in the data, e.g. in the {\small \it XMM-Newton}\ 2001 and {\small \it Suzaku}\ 2007 spectra, raise the confidence one has in the model, even if they do not result in superior statistical fits.
In fact, the 2001 {\small \it XMM-Newton}\ spectrum is perhaps the hardest to fit and we find the partial covering model essential to even obtain an adequate description of the continuum.
In the following section we elaborate on the model for this observation that is derived from both the {\small EPIC~PN}\ and {\small RGS}\ data.

\subsection{The 2001 RGS spectrum revisited}
\label{sec:rgs01}

The 2001 {\small \it XMM-Newton}\ observation is the only observation of \pds\ to provide identifiable absorption lines in the gratings.
The least ambiguous absorption features in the 2001 {\small RGS}\ spectrum are observed in the 11.5 -- 14.0~\AA\ range, and in particular there appears to be a deep and broad absorption trough between 13.5 -- 14.0~\AA.
We re-analyze the {\small RGS}\ spectrum of \pds\ from the 2001 observation with the same absorption models as used above for the CCD data.
The method used here is not very different from that of \citet{reeves03}, who used {\small \it XSTAR}\ tables.
We find that the ionization parameter of $\log \xi = 2.6$ (cgs units) given by \citet{reeves03} for the {\small RGS}\ spectra
produces on top of the 14~\AA\ feature other strong lines that are not seen in the data.
In order to produce only a few features, we need to increase the ionization parameter to $\log \xi \approx 3.0$, to ensure that most species are fully ionized and only a trace of Fe-L remains.
Indeed, we are able to find a model with $\log \xi = 3.1$ that fits the {\small RGS}\ absorption features,
and is marginally consistent with the fit to the {\small EPIC~PN}\ data obtained in Section~\ref{fit_results} (Table~\ref{table:fit}) that is not as sensitive to narrow line features.
The relevant part of the {\small RGS}\ spectrum along with the model is presented in Fig.~\ref{rgs01}.
Unfortunately, {\small RGS} 1 does not provide data between 11.5 -- 13.75~\AA, due to a failed chip.
In Fig.~\ref{rgs01}, thus, only {\small RGS} 2 is shown, although both {\small RGS} s are used in the fit and are consistent with each other.

According to the present model, several absorption features are shifted by $z = 0.13$ and can be tentatively identified in Fig.~\ref{abs_models}.
We identify the wide trough between 13.5 and 14.0~\AA\  predominantly with Ne$^{+9}$ Ly\,$\alpha$ ($\lambda _\mathrm{rest} = 12.134$~\AA) that is broad ($v_\mathrm{turb} \approx\ 2500~\kms$) and blended with the resonant ($f = 1.24$) 2p -- 3d line of  Fe$^{+20}$ ($\lambda _\mathrm{rest} = 12.284$~\AA).
The strength of the Ne$^{+9}$ Ly\,$\alpha$ line may indicate an overabundance of Ne, although no abundances could be reliably constrained.
The Ne$^{+9}$ Ly\,$\beta$ line in this model falls at 11.6~\AA\ ($\lambda _\mathrm{rest} = 10.239$~\AA), just next to a chip gap in {\small RGS} 2 (and where {\small RGS} 1 is still inactive), so it is not obvious in the spectrum.
Another relatively strong line is found at 12.01~\AA\ and identified as the Fe$^{+23}$ 2s -- 3p doublet ($\lambda _\mathrm{rest} = 10.621, 10.664$~\AA).
Finally, the model plotted in Fig.~\ref{rgs01} also predicts absorption by Fe$^{+22}$ at 12.4~\AA\  ($\lambda _\mathrm{rest} = 10.982, 11.021$~\AA), which is not clearly identified in the spectrum,
but consistent with the data uncertainty.
This blend could be overestimated in the model if the ionization parameter or the ionization balance are slightly off.
These high charge states of Fe give an idea of the highly ionized state of the absorber.

The outflow velocity resulting from the aforementioned tentative line identifications as due to a shift of $z = 0.13$ is $v_\mathrm{out}/c = 0.13 - 0.184$, or $v_\mathrm{out} = -16,000~\pm\ 1,500~\kms$, slower than found by \citet{reeves03}, but consistent with the velocities seen for H Ly\,$\alpha$ absorption in the {\small UV}.
The connection to the {\small UV}\ absorber is puzzling since no high-ionization absorption lines were detected there \citep{obrien05}.
The determination of the outflow velocity obviously depends on the correct identification of the absorption lines.
Except for the 14~\AA\ feature, other identifications are marginally significant, and thus the outflow velocity derived mostly from one feature will always remain ambiguous.
The Fe-K edge observed with {\small EPIC~PN}\ at 8~keV still requires a high velocity of $\sim 50,000$~\kms.
This leaves the present velocity as well as that of \citet{reeves03} possible.
In any event, the CCD spectra that are of higher statistical quality and that were discussed in the previous section can not distinguish between the two interpretations of the {\small RGS}\ data.
Fig.~\ref{rgs01} also highlights emission lines produced by the reflection model, which appear to be consistent with the {\small RGS}\ data. The brightest line is at 17~\AA, which is the 2p -- 3d resonance line of Fe$^{+16}$ (redshifted with the outflow by $z$ = 0.13).
Two additional narrow features that are not reproduced by the model appear in the {\small RGS} 2 spectrum of Fig.~\ref{rgs01}, namely at 15.18~\AA\ and at 17.90~\AA.
The 15.18~\AA\ line appears in both {\small RGS} s and corresponds to 13.43~\AA\ in the outflow frame, which could be the 1s -- 2p resonant line of Ne$^{+8}$.
The 17.9~\AA\ line is totally absent from the equally good spectrum of {\small RGS} 1 (not shown) and can be discarded.

\section{Conclusions}
This paper presents the {\small \it XMM-Newton}\ observation of \pds, which took place in September 2007,
 and attempts to generalize its results to the broader context of four other CCD-quality observations of the quasar acquired over the past decade, each one of them revealing a spectrum quite remarkably different from the others.
In a sense, the 2007 {\small \it XMM-Newton}\ spectrum is the most straightforward to interpret, as no unambiguous absorption is present.
On the other hand, owing to the lack of ionized absorption, a significant reflection component can be discerned.
Global fits to the spectrum suggest it may be outflowing with respect to the quasar's rest frame,
although this result is less robust that the mere existence of a reflecting medium.
Since an absorbing outflow has been identified in \pds,
a natural conjecture is to associate the reflector with outflow segments outside the line of sight.
The small solid angle coverage of the source of $\sim$~20\% found for the reflecting medium is consistent with this notion,
although the assumption of a single scatter, perfect reflector are clearly an over simplified picture of a more realistic reflecting outflow.
The velocities required to model the reflecting material are in the range of $v/c$ = --0.04 to --0.08, which is roughly comparable to the blueshifted absorption measured in the {\small UV}\ and to the interpretation of the 2001 {\small RGS}\ spectrum.  A separate component is needed to explain the much faster Fe-K absorption, observed e.g. with {\small \it Suzaku}.

The historical spectra of \pds\ point to a complex nature of the source and complex absorption.
We tested whether all spectra can be explained by a partial covering outflow model that both absorbs and reflects the central source and obtained mixed results.
This type of model is sufficiently flexible to produce a wide variety of spectra, but is only partially successful in reproducing those of \pds.
While the different over all spectral curvatures of \pds\ are produced by varying the fractional coverage of the source essentially from zero to unity, the spectral fits are not always statistically acceptable, and some narrow features predicted by the models are discrepant with the observed spectra.
These features vary in the data on time scales from days to years.
The reflection component can explain some of the emission that is excessive of the power law continuum. In the 2007 epochs, it provides a good fit to the Fe-K emission, but in other epochs, its  details of the soft emission below 2~keV do not always match the data very well.
Future \x\ instruments that would provide high S/N spectra on short time scales are imperative to further advance the study of such outflows.

\begin{acknowledgements}
EB acknowledges funding from
a NASA {\small \it XMM-Newton}\ Guest Observer grant and from
NASA grant 08-ADP08-0076.
SK is supported at the Technion by the Kitzman Fellowship and by a
grant from the Israel-Niedersachsen collaboration program.
\end{acknowledgements}

redpajama_set_name: RedPajamaArXiv


The upcoming India-US 2+2 talks — an apex bilateral meet in New Delhi next week — is not just 'historic' but will throw up a set of 'very concrete outcomes' which will serve as "enablers" for the India-US relationship well beyond the high optics of 6 and 7 September, a US Defence Department official familiar with the preparations said in Washington DC Wednesday. Headlining the US approach to the India-US talks are two words: "operationalising" and "enabling" the relationships that already exist on the basis of years of work by multiple governments on both sides.
Randall Schriver, Assistant Secretary of Defence for Asian and Pacific Security Affairs at the US Department of Defense, made these comments during an hour-long fireside with Ashley Tellis at the Carnegie Endowment for International Peace focussed specifically on the India-US 2+2 scheduled for next week in New Delhi.
US defence secretary James Mattis and Secretary of State Mike Pompeo are scheduled to meet India's foreign minister Sushma Swaraj and defence minister Nirmala Sitharaman on 6 September. Mattis and Pompeo will also call on Prime Minister Narendra Modi.
The US team gearing up for the talks, according to Shriver, is plotting the dots on the basis of the speeches that Modi and Mattis gave at the Shangri La dialogue. Schriver said the upcoming talks will be very different from bilaterals where the energy and enthusiasm dissipates after the actual meeting itself and instead be one that "enables" a more substantive and continuing relationship between the countries' top bureaucrats well after the apex level talks. "There are times when we talk, meet and go away, this is not going to be one of those," Shriver said.
"At the core is our belief that we're promoting a positive, affirmative vision for the region. It's not necessarily anti-anybody or counter-anybody. It's just affirming the principle of a free and open Indo-Pacific. The core of that is we believe countries should have sovereign control to make decisions free from coercion, pressure... and have free, open, reciprocal trade relationships. We mean commerce, navigation, broad participation economically. We know there are threats to that from predatory economics but we don't seek influence or control."
"Our interests are very compelling on the defence side. We're quite bullish at the US Department of Defense. We're really the beneficiaries of decades of great work, the Bush administration, working through the civil nuclear deal, the creation of a major defence partner label during the Obama administration — it's been evolutionary in nature. We benefit from leadership on both sides willing to take some risks. We'll be able to navigate this and come out on the other side and be able to say we were able to build on all that came before.
"I would suggest lay side by side Secretary Mattis' speech at Shangri La and Prime Minister Modi's speech at Shangri La. We are not searching for common ground and convergence — there's a lot of that already. Our goal is really to operationalise that with India as a partner. The specifics will take form, some of that will be in the defence area, development assistance area. That's what we are working on.
"If you're against free and/or open, then there's an onus there to explain what you don't like about it. It's not so much about countering any particular country but China's behaviour, things they've articulated…. They're very clear. They're articulating a very different vision and that's obvious in their economic strategy, in their Belt and Road Initiative — the coercive approach to influencing the politics of others. The world we live in, it's allowing others to coalesce around the resistance to this and that's an upside. We are more dependable partner in the Indo-Pacific — that's what we'd rather say than saying don't do this or that with China. That's unrealistic, given China's size, influence and geography. China will certainly be a factor in whatever we do going forward.
"The relationship has matured to the extent that we can think of how we can together address problems of third parties. We will talk of developmental assistance and common effort for third parties. That is where our relationship is. True in the security area as well. We exercise to improve readiness and real world possibilities. Multilateralising those opportunities is part of the 2 + 2 talks.
"In my opinion, the Quad began on 26 December, 2004 — which was the day of the great tsunami in Southeast Asia when the four countries that responded were India, Australia, Japan and the US. We responded because we are like minded and felt the compelling need to help and had the willingness to cooperate. In a way, the Quad was born in reality before it was born as a concept. Now, we're looking at this as a potential vehicle to see how it could promote a range of our interests in the Indo-Pacific. It'll move at a pace and scope that all four are comfortable with and that's been the constraint historically, right. So, it's not at the pace we may like but we'll get to it, eventually.
"We note that India has a better relationship with China this year than the last… The last year was pretty bad. We want a good relationship with China too. We have some clear areas of disagreement on the South China Sea, on Taiwan... but we want a better relationship with China. So we'll work with our friends in India and try to navigate all that."