November 23, 2006 By Emma Marris This article courtesy of Nature News.
Soils lacking sulphur may increase carcinogens in crops.
Not enough sulphur in the wheat can spell 'probable carcinogen' in the bun, according to new research.
Researchers first discovered traces of acrylamide, a chemical linked to cancer and other possible ill effects, in baked and fried goods in 2002, to universal dismay1. Since then, food scientists have spent untold hours trying to reduce the amounts of this chemical in foods. That's hard to do without losing the lovely flavour of baked goods: the compound is made by the reaction that forms the tasty golden brown crust on a loaf of bread.
A group led by Donald Mottram, professor of food biosciences at the University of Reading, UK, approached the problem not by looking at how acrylamide is produced in the cooking process, but how the precursors to the nasty chemical wind up in wheat in the first place.
They report in the Journal of Agricultural and Food Chemistry that wheat grown in fields deficient in sulphur have much higher concentrations of asparagines an amino acid that, along with sugars, forms acrylamide during cooking2.
Sulphur deficiency in wheat fields is widespread around the globe: 23% of UK fields are said to be sulphur deficient. According to Mottram, making sure that crops have plenty of sulphur might go some way towards reducing acrylamide in foods. And it would do so without changing the flavour.
"The manufacturers of biscuits and cakes and breads and crisps they have modified their processes wherever possible," says Mottram "But if we can get the levels of asparagine lower in plants, there won't be as much acrylamide there to start with."
The team grew wheat in pots with identical conditions, bar the sulphur content. Those with a sulphur deficiency made wheat that, when milled and cooked, had 4.7 times the amount of acrylamide as the plants that could gorge on the element. Wheat in field trials showed an even more dramatic response. The sulphur-starved wheat made cooked products with 6.3 times as much acrylamide.
Nigel Halford, a co-author and crop scientist at Rothamsted Research in Harpenden, UK, says they think this is because the production of seed storage proteins decreases when a plant is stressed by sulphur deprivation. The nitrogen taken up by the plant then accumulates as asparagine instead.
Halford says other stresses on the plant, such as heat or nitrogen deficiency, may have a similar effect they are keen to study this to find out.
Richard Stadler, of Nestlé in Orbe, Switzerland, is pleased that research on acrylamide has expanded past the kitchen. "This work will contribute significantly to a better understanding of the impact of agronomic factors a major gap in our knowledge with regard to acrylamide mitigation," he says.
Tareke E., et al. JAFC, 50 . 4998 - 5006 (2002).
Muttucumaru N., et al. JAFC, doi:10.1021/jf0623081 (2006).


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Three takeaways from Texas' brutal loss at Maryland
Photo Credit: Katie Bauer | Daily Texan Staff
Published on September 1, 2018 at 9:04 pm Last update on September 3, 2018 at 8:43 pm
By Ross Burkhart
It may be a new season for Texas, but it was the same result as last year's opener — an undisciplined Longhorn team getting upset by underdog Maryland.
Saturday's 34-29 loss had plenty of defining moments, including key fourth-quarter turnovers, a one hour and 26 minute rain delay and the defense's inability to force turnovers.
Here are three of the biggest takeaways from Texas' season opener:
Fourth-quarter execution is still a problem
The Longhorns were nearly mistake free on the offensive end. Then, the fourth quarter began.
Sophomore quarterback Sam Ehlinger took the field with 6:45 to go in the game. Two players later, a costly interception saw the Maryland offense regain possession.
On the next drive, a fumble from Texas running back Tre Watson near the 50-yard line halted another opportunity for the Longhorns to take control late in the game.
To the defense's credit, Ehlinger and the Longhorns had a third and final opportunity to complete a comeback, only to have it stripped away by junior Maryland defensive back Antoine Brooks Jr. after a an interception on 3rd-and-10.
It's a story Texas fans are all too familiar with. Late turnovers defined the outcome for the Longhorns.
Ehlinger, who threw for two touchdowns over the first three quarters, said that his game mimicked how the team performed as a whole.
"I thought my individual performance kind of embodied how we did as a team overall," Ehlinger told Longhorn Network after the game. "We started slow, middle of the game, we finally found our stride and who we needed to be. Then, at the end, we didn't finish so I think that resembles it pretty well."
Executing in late-game situations is an issue Texas desperately needs to correct if they want to have any shot at getting close to the top of the Big 12 this season.
Orlando's defense struggles to take away the ball
Despite having one of the top defenses in the Big 12 last season, the Longhorns struggled to create turnovers. Saturday didn't prove very different as Texas failed to record a single takeaway.
Early on, the lack of pressure showed as Maryland quickly ran out to a 24-7 lead. Texas recovered down the stretch but eventually gave up 34 points by the end of the game.
The defense's failure to keep the Terrapins out of the end zone was too much for the Texas offense to overcome. After the game, senior defensive tackle Chris Nelson said that he didn't approve of the defense's performance.
"For me, my standpoint, I don't like it," Nelson said. "I know we can play better than that and we will play better than that."
Coaching staff emphasizes running game
Another question following head coach Tom Herman and the coaching staff going into Saturday's game was the amount of run plays that will be called this season.
Last season's offensive personnel consisted of a revolving door at the running back position, but one of the more positive aspects from Saturday's game was the 27 carries by four different running backs. Watson recorded 57 yards on 12 carries and freshman Keaontay Ingram tallied 37 yards on six carries in his first game in burnt orange.
The numbers aren't eye-popping, but the decision to stick with the run, even when the team found themselves down by three scores, is promising.
The Longhorns showed on Saturday that there's at least two runners they feel comfortable with. If they want to ease the questions about Ehlinger's play, Herman should continue to get the running backs involved early and often each week.
Texas kicks off a three-game stretch at home next weekend as the Longhorns will take on Tulsa.

redpajama_set_name: RedPajamaCommonCrawl


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Nanterre adds depth with Bouquet
May 25, 2019 by Eurocupbasketball.com Print
Nanterre added depth to its squad by signing versatile swingman Damien Bouquet to a three-year deal. Bouquet (1.96 meters, 25 years old) arrives from second-division ALM Evreux Basket, where he spent the past two seasons. He averaged 9.7 points, 6.1 assists and 3.6 rebounds last season. Bouquet made his professional debut at Charleville-Mezieres after growing up with Strasbourg. He is now set to make his 7DAYS EuroCup with Nanterre.
Nanterre brings back shooting guard Butterfield
Nanterre 92 added firepower to its roster by signing shooting guard Spencer Butterfield to a one-year deal, the club announced Friday. Butterfield already played for Nanterre...
Nanterre lands playmaker Chery
Nanterre 92 added a new floor general to its roster, none other than Kenny Chery, who signed a one-year deal with the French powerhouse on Wednesday. Chery arrives from...
Nanterre adds do-it-all forward Smith
Nanterre 92 has announced the arrival of a new forward, Taylor Smith, for the team's return to the 7DAYS EuroCup after four seasons. Smith is a six-year pro who has played two...


Dirk Schaper, K Gerlach. Epididymal Cyst with Testicular Retention, Hydatid and Hydrocele. PedRad [serial online] vol 5, no. 7.
Presentation because of retention of the testes at 8 weeks of age. Right hemiscrotum was hypoplastic, the testis itself is, however, well-palpated in the right inguinal region. There is somewhat resistence. On the other side, the scrotum is well-developed with discrete testicular hydrocele. Beta-HCG and Alpha-Fetoprotein were unremarkable.
Epididymal cysts are generally benign and spontaneously regress. They are often a chance finding of a sonographic examination of the male genitalia. They can, however, cause symptoms - especially when they are large and give the patient a weighted-down feeling. One finds epididymal cysts in children whose mothers were treated with Diethylstilbestrol (DES). But also children who have testicular retention, cystic fibrosis and von Hippel-Lindau's Disease have increased incidence of epididymal cysts. A connection with the autosomal-dominant passed on disease of Polycystic Kidney Disease is being discussed.
Wollin et al. saw developmental rudimentary structures of the epididymis which had no connection to the tubule system of the epididymis.
Others see a hormonal cause as a leading cause and categorize the epididymal cyst as a testicular dysgenesis.
The increased incidence in connection to a maldescendent testis is not able to be explained at this time. How epididymal obstruction or an abnormal hormonal reaction are the causes is still unclear.
Ultrasound 1: A mass which is low in echoes in the epididymal head in testicular retention and testicular hydrocele.
Ultrasound 2: 6,3 x6,7 mm mass of the right epididymal head.
Ultrasound 3: Opposite side you see a 1,5mm large structure by the epididymis which is free of echoes.
Ultrasound 4: Opposite side you see a 1,5mm large structure by the epididymis which is free of echoes with a testicular hydrocele.
Because of the unclear mass and the danger of torsion with the testicular retention, we decided to operate. The epididymal cyst was scraped out, the hydatide was removed and the testes were pexated. We also found kidney tissue in the spermatic cord during surgery.
The sonographically seen hydatide of the opposite side was not operated on.
Epididymal Cysts in Children: Natural History.
Abberant epididymal tissue: a significant clinical entity.


The Zoology Collection is inspired by the wonderful variety of life on our planet, with the usual quirky charm and beautiful illustration that we are known for. This design features a lovely, pink dodo. Each card is printed on high quality, textured board and is 150 x 150mm in size. It is supplied cello wrapped with a white envelope and is blank inside for your own message.


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Wikipedia ProfilesExpand
Ibrahim Magu is a 59-years-old Nigerian former acting chairman of EFCC from the Nigeria. his estimated net worth is $1 Million to $5 Million Approx. Jump into read his life Facts, Wikipedia and biographies Details
1 Ibrahim Magu Biography – Wiki
2 Fast Facts You Need To Know
3 BirthName, Nickname, and Profession
4 Age, Birthdate, Religion, and BirthPlace
5 Height, Weight, And Body Measurements
6 Ibrahim Magu Personal Life, Spouse, Wife
7 Ibrahim Magu Net Worth
8 Twitter, Facebook, and Instagram
Ibrahim Magu Biography – Wiki
According to the wiki and biography of Ibrahim Magu was born on 5 May 1962 in Nigeria. let's check out the Ibrahim's personal and public life facts, Wikipedia, bio, spouse, net worth, and career details.
Fast Facts You Need To Know
Magu remains unconfirmed as the Chairman of EFFC which is one of the challenges and controversies being faced by the administration of President Muhammadu Buhari on appointments and nominations confirmation. The Police Service Commission (PSC) on Friday, 28 April 2018 announced the promotion of 18 senior officers after her 27th Plenary Meeting which ended in Abuja where Magu was promoted to the rank of a full commissioner from deputy commissioner.
At the end of the 8th Regional Conference of Anti-Corruption Agencies in Commonwealth Africa held at Transcorp Hilton (Abuja, Nigeria) on 19 May 2018, Magu has emerged their new chairman. His appointment was the highpoint of a five-day regional conference with the theme: "Partnering Towards Assets Recovery and Return".
On May 29, 2018, the EFCC announced that 603 Nigerian figures had been convicted on corruption charges since Buhari and Magu assumed their offices in 2015. The EFCC also announced that for the first time in Nigeria's history, judges and military officials were prosecuted.
On 4 August 2008, he was arrested following allegations that police discovered EFCC files and a computer containing classified documents at his Abuja residence. Presently, he is a member of the investigative committee convened by National Security Adviser (NSA), Babagana Monguno on the orders of President Muhammadu Buhari to probe the procurement of arms in the Armed Forces from 2007 till now.
Ibrahim Magu (born 5 May 1962) is a Nigerian police officer who was appointed Acting Chairman of the Economic and Financial Crimes Commission (EFCC) on 9 November 2015 after chairman Ibrahim Lamorde (who has earlier served twice) was sacked by President Muhammadu Buhari. Both Lamorde and Magu served during Nuhu Ribadu's time at the anti-graft agency and were also credited with part of the success Ribadu recorded in his time.
Magu was born on 5 May 1962 in Maiduguri, Borno State. He attended Maiduguri's primary school (from 1969 to 1975), Waka Biu's Secondary School from 1975 to 1980 and Ahmadu Bello University, Zaria from 1982 to 1986 where he graduated with a B.Sc Accounting. After the completion of his National Youth Service Corps, he served in various Ministries and Departments in the Borno State Government as an Accountant and rose to become a Zonal Accountant before he voluntarily resigned to join the Nigeria Police Force as an Assistant Superintendent of Police in 1990. He was the Coordinator, Nigeria Police Building Society before moving on to Special Fraud Unit (SFU) of the Nigeria Police Criminal Investigations Department (CID) where he served as a team leader in charge of Financial Crimes, Money Laundering and Advance Fee Fraud investigation.
BirthName, Nickname, and Profession
So first, let's take a look at some personal details of Ibrahim, like name, nickname, and profession.
Real Name Ibrahim Magu
Nickname Ibrahim
Profession former acting chairman of EFCC
Age, Birthdate, Religion, and BirthPlace
Age (2021) 59 Years
Birthplace Maiduguri
Date Of Birth 5 May 1962
Sunsign Gemini
Hometown Maiduguri
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In Pound: not available
Ibrahim Magu Personal Life, Spouse, Wife
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Father Not Available
Mother Not Available
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Girlfriend Update Soon
Ibrahim Magu Net Worth
The Ibrahim Magu Estimated Net worth is $80K – USD $85k.
Monthly Income/Salary (approx.) $80K – $85k USD
Net Worth (approx.) $4 million- $6 million USD
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import { resources } from '../../../../common/api-client';

export default function AchievementsScreen(config) {
	const template = `

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		leave() {
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redpajama_set_name: RedPajamaGithub


Prior to joining ML Strategies, Jenny worked as a legislative assistant at a prominent international law firm. There she closely followed pieces of legislation related to criminal justice reform, cyber-security, transportation, and housing, in order to provide real-time updates to lobbyists and clients. Previously, Jenny worked as a legislative correspondent for U.S. Senator Chuck Grassley (R-IA) where she participated in lobbyist meetings and agency briefings, organized panel discussions, and assisted in composing floor speeches for the Senator.
Jenny recently graduated with her Masters in Congressional and Presidential Studies from the Catholic University of America. During her time at Catholic, Jenny was named a Bryce Harlow Fellow, a prestigious award for students who pursue careers in professional advocacy. As an undergraduate, Jenny was a University Scholar and was awarded both the Diane Jones Meier Award and the Fowler Award for Leadership for her work in the political science department. She served as a policy intern for U.S. Senator Deb Fischer (R-NE) and as a library intern for the U.S. Secretary of the Senate.
Read about recent TCPA cases and FCC comment periods on automatic telephone dialing systems, call blocking technologies, and a proposed emergency use exemption to the TCPA.
In this issue, we look at industry comments on the FCC's report on robocalling and efforts to urge the agency to reconsider its reassigned numbers database proposal. In addition, we examine a recent circuit split on what constitutes an automatic telephone dialing system (ATDS) in the Third and Ninth Circuits and what that means for TCPA defendants. The split follows the D.C. Circuit's May 2018 decision in ACA International v. Federal Communications Commission, which set aside the FCC's "unreasonably expansive interpretation" of what constitutes an automatic telephone dialing system.
This issue provides insurance information for companies facing TCPA lawsuits and identifies the types of policies and provisions that may offer coverage. You will also find an update on the status of the proposed reassigned numbers database as well as information about a new FCC Public Notice, released August 10. Comments on the Public Notice are expected to lay the groundwork for the FCC's next major action on call blocking and methods to eliminate illegal robocalls.
This issue includes an update on activity at the FCC, specifically the agency's progress in evaluating comments received in several ongoing TCPA proceedings. In addition, in our Class Action Update, we look at the current understanding of what constitutes an ATDS and why, in the wake of ACA International, it may be more difficult for plaintiffs to demonstrate that the companies they are suing used ATDS devices.
In this issue, we look at recent TCPA-related activity at the FCC, including the agency's reevaulation of some TCPA rulings as well as a notable fine levied against a robocaller for malicious spoofing. In addition, in our Class Action & Litigation Update, we look at recent district court rulings offering different interpretations of what constitutes an ATDS, and consider where this split between the circuits leaves TCPA defendants.
This month we consider the Ninth Circuit's pending Crunch ruling and how the decision may affect parties defending TCPA cases. You'll find the story in our Class Action & Litigation Update. Our Legislative Update offers a quick review of the recent US House and Senate hearings on illegal robocalls. For a roundup of TCPA-related developments at the FCC, please see our Regulatory Update.
Every month, robocalls make up the majority of Do Not Call registry complaints at the Federal Trade Commission (FTC). The FCC estimated that in March 2018 approximately 3 billion robocalls were placed. In an effort to combat these illegal robocalls, the Senate Commerce Committee and the House Energy & Commerce Committee each held a hearing regarding these illegal robocalls and asked witnesses for ideas on how to combat this rampant problem.


At ResilienceCon 2019, we are proud to provide eight scholarships for promising scholars and promising advocates.
The deadline to apply for a Promising Scholar or Promising Advocate scholarship has passed.
Scholarship winners are expected to attend the entire conference, April 14-16, 2019.
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(1859–91). French neo-impressionist painter Georges Seurat is the ultimate example of the artist as scientist. He spent his life studying color theories and the effects of different linear structures. His 500 drawings alone establish Seurat as a great master, but he will be remembered for his technique called pointillism, or divisionism, which uses small dots or strokes of contrasting color to create subtle changes in form.
Georges-Pierre Seurat was born on Dec. 2, 1859, in Paris. He studied at the École des Beaux-Arts in 1878 and 1879. His teacher was a disciple of Jean-Auguste-Dominique Ingres. Young Seurat was strongly influenced by Rembrandt and Francisco de Goya.


text:
Ugo av Farfa, född omkring 973, död 1039, var abbot av benediktinklostret Farfa från år 998 till sin död. Under Ugo upplevde Farfa en av sina blomstringsperioder.

Källor

Italienska benediktiner
Italienska abbotar
Födda 973
Avlidna 1039
Män

redpajama_set_name: RedPajamaWikipedia


Highland Park is located in Middlesex County, within New Jersey. The approximate center of this city is: 40.5006, -74.4271.
We have many types of places to explore in and around Highland Park, Middlesex County, New Jersey!


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Tempestuous relations: Brexit and UK future drone developments
Tempest concept image
In May 2017, Chair of BAE Systems, Sir Roger Carr, blithely insisted at the company's AGM that Brexit would have no impact whatsoever on the on-going development of the new Anglo-French advanced combat drone. "We will still be working with the EU on defence, certainly in terms of fighting terrorism, and we can preserve our relationship with France in developing the next generation of unmanned aircraft," he told shareholders.
Just two months later Carr had to eat his words as a major realignment of European aerospace programmes saw France sign a surprise agreement with Germany to develop a new future combat aircraft. While both BAE Systems and France's Dassault tried to argue that research work on the Anglo-French combat drone could continue in parallel with the new German deal, silence about the programme at the Anglo-French Summit in January 2018 confirmed that the drone programme was in serious trouble due to uncertainties around Brexit.
Seemingly in response, Defence Secretary Gavin Williamson unveiled a full-scale model of a potential new British combat aircraft – Tempest – alongside publishing the UK's Combat Air Strategy at the Farnborough Air Show in late July. The new initiative, as Defense News put it, "essentially replaces the Anglo-French FCAS program."
Like many projects at the pipe dream stage, we are being told that the proposed new aircraft will be utterly amazing and capable of doing almost anything:
"An operational platform could be manned or unmanned, and capable of deploying swarming munitions and carrying a laser directed-energy weapon," reported Flight Global;
"An artificial-intelligence-driven autonomous flight system would allow the aircraft to fly without a pilot on board, coordinating instead with other fighter jets, said Wired;
"Tempest will use artificial intelligence and machine learning to ensure its weapons hit their targets. It will also carry energy weapons that fire concentrated bursts of laser, microwave or particle beams to inflict damage." according to The Sun.
Graphic published about the potential wonders of Tempest
While Tempest received a great deal of media coverage, it is hard to see, at this stage, much substance behind the PR. "None of it is real. It's wishful thinking" Labour MP and member of the Defence Select Committee, Ruth Smeeth, told the Financial Times. Other analysts argued that it was perhaps "more significant politically than technologically or aeronautically."
The Franco-German Future Combat Air System and the new Tempest project are in addition to the European MALE project currently being developed by Airbus and Dassault and it is very hard to see how all of these programmes could be sustained financially. Its seems far more likely that this is all political posturing and positioning ahead of some future alignment post-Brexit. Importantly, despite talk of government and industry 'pledges' of £2bn, there will be no financial decision about government spending on Tempest until 2025. In the current climate that is light years away.
As Louise Brooke-Holland notes in her House of Common briefing 'From Typhoon to Tempest'
"Whether the UK eventually partners France and Germany, or forges ahead on a separate programme with other partners, won't become clear for some time. It is quite possible the three nations will eventually work together."
Besides the smoke and mirrors on whether the UK could actually afford economically or politically to proceed independently of its European allies on a new programme, Justin Bronk of RUSI nails the other inherent contradiction in the project on the head:
The Tempest will supposedly be flyable by a pilot in the cockpit or capable of operating as a drone – an arrangement known as 'optionally manned' in aviation circles. However, most of the design advantages gained by eliminating the need for an onboard crew are clearly lost in an optionally manned design. It still requires a cockpit, life support systems, physical controls and an instrumentation/information display system for the pilot, all of which add weight, complexity, reduce the space available for fuel, weapons and sensors, and the need for a canopy fairing limits how stealthy the airframe can be made. Perhaps more importantly, if pilots are to be trained for the Tempest, this will require expensive peacetime flying to train and maintain pilot proficiency. The fact that a UCAV can, in theory, stay on the ground, with operators trained simply with simulated aircraft except during actual operational missions, is a key potential cost-saving feature of unmanned alternatives to fast jets, but this would be largely lost with an optionally manned type. On the other hand, while the ability to fly high-risk missions unmanned, to reduce the risk to human pilots, is theoretically useful, the extra electronic complexity and programming risk needed to develop a combat aircraft capable of operating in complex and contested environments without a pilot on board is still required.
While Gavin Williamson will no doubt be very pleased with the press coverage that Tempest has received, and Brexiteers will be convinced that Britain can simply go it alone in developing the new aircraft, the reality is that like many other projects, the UK's involvement in developing a future drone appears to be on hold pending negotiations around Brexit.
UK Drones - Future plans BAE Systems, British drones, Dassault, France, funding, Tempest Leave a comment
← Book review: 'Army of None: Autonomous weapons and the future of war' by Paul Scharre
"Here's their actual stories, make of them what you will." Dr Peter Lee on 'Britain's Reaper Force' →


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Review: Marwencol DVD
– April 8, 2011Find Others: DVD, Movie, ReviewGet More: Cinema Guild, Documentary, Independent Film
STUDIO: Cinema Guild | DIRECTOR: Jeff Malmberg
RELEASE DATE: 4/12/11 | PRICE: DVD $29.95, Blu-ray $34.95
BONUSES: deleted scenes, additional story sequences, Mark's reactions, intro by film critic Elvis Mitchell, collectible Marwencol mini-print
SPECS: NR | 84 min. | Documentary | 1.85:1 widescreen | Dolby Digital 2.0/DTS-HD 2.0
RATINGS (out of 5): Movie | Audio | Video | Overall
Mark Hogencamp details the miniature town of Marwencol.
A truly unique documentary that has won accolades wherever it has played, Marwencol centers on Mark Hogencamp, an upstate New York man who suffered brain damage after he was brutally attacked by five men in a neighborhood bar in 2000. When his health insurance company stopped paying medical bills for rehabilitation, he began his own therapy by building a miniature version of a World War II village in Belgium, the fictional Marwencol. He populated it with era-appropriate doll characters based on people he knows and photographed his striking, realistic-looking results. Eventually, his long-term project was discovered by an art magazine, prompting a gallery show in Manhattan that both interested and scared the shielded Hogencamp.
Inspirational, unsettling and just plain odd, Marwencol is fascinating from the first movie frame to the last, with some final reel revelations that are sure to surprise. Gruff, chain-smoking and somewhat guarded, Hogencamp isn't the most personable guy all the time, but his human qualities are what make him a downright fascinating and complex character.
Debuting film director Jeff Malmberg followed Hogencamp over the course of four years, capturing his subject with video and super 8mm cameras, and chronicling the stories that Hogencamp weaves about Marwencol village and his miniature-sized friends. Malmberg has made a poignant film that touches on such subjects as mortality, the health insurance crisis, the nature of art and the right to privacy, while being entertaining at the same time.
Both the Blu-ray and DVD offer an identical slew of extras. Most indispensable are the 17 deleted scenes that shed additional light on Hogencamp's life and art. Amongst these are worthwhile sequences that find Hogencamp dressing his dolls, discussing his feelings about women and his continuing therapy, and attending his own art opening.
The discs also include seven additional, well-detailed Marwencol story sequences that transport viewers even further into the recesses of their creator's healing mind.
Buy or Rent Marwencol
DVD | Blu-ray DVD | Blu-ray DVD | Blu-ray
Review: Poliwood DVD
Review: Howard Zinn You Can't Be Neutral on a Moving Train DVD
New Release: Marwencol Blu-ray and DVD
Review: 9000 Needles DVD
DVD Review: The Other F Word
About Irv
Irv Slifkin has been reviewing movies since before he got kicked off of his high school radio station for panning The Towering Inferno in 1974. He has written the books VideoHound's Groovy Movies: Far-Out Films of the Psychedelic Era and Filmadelphia: A Celebration of a City's Movies, and has contributed film reportage and reviews to such outlets as Entertainment Weekly, The Hollywood Reporter, Video Business magazine and National Public Radio.
Mark Wencol
Posted April 11, 2011 at 2:17 PM
That's one wacky dude!


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\section{Introduction}\label{intro}
The study of  gravitationally lensed quasars is relevant both to cosmology and  to the determination of the total mass in (lensing) galaxies. Time delays between multiple quasar images depend both on the mass distribution of the lensing galaxy and on the Hubble parameter, H$_0$ (Refsdal, 1964). The translation of an observed time delay into a value of H$_0$\, requires the modelling of the surface mass density of the lens.  For that purpose, geometric and photometric constraints are needed such as: (a) spectroscopic redshifts for both the source and the lens components and (b) accurate relative positions of the lensed images and of the lensing galaxy. Additional constraints to be used are the flux ratios (FRs) between the quasar images. Indeed, the FRs are equal to the magnification ratios at the image positions, and hence depend on the mass distribution of the lens. However, the contribution of the lens (lensing galaxy and environment) must be disentangled from other sources of flux variation such as:  differential galactic extinction, intrinsic quasar variability, microlensing and/or millilensing (de)magnification, all phenomena which have different time scales and wavelength dependencies (see e.g. Anguita et al. 2008 for more details). In the case of radio loud quasars this is rather straightforward, yet it does not apply to the whole quasar population. For optically selected quasar, the separation of the different sources of flux variation is more complex. In spite of this complexity, one must attempt it to derive values of the image FRs genuinely related to the strong lens. In the case of doubly imaged quasars (which constitute $\sim$60\% of the strongly lensed quasars known so far), it is particularly important to use the FR to constraint the lens mass model, as these systems are  naturally the least constrained. \\
In this paper we report on new observations of  the lensed quasar QJ~0158-4325, and on a model of the lensing system. The quasar and the  datasets relevant to our study are presented in $\S$~\ref{theqso}. In $\S$~\ref{deconvsec}, the spectra and image deconvolutions are discussed. We model the lens in $\S$~\ref{simple}. Conclusions are given in $\S$~\ref{dandc}.  \\
We assume a WMAP type cosmology (Spergel et al. 2003, 2007): $H_0$=73~km~s$^{-1}$~Mpc$^{-1}$, $\Omega_m$=0.3 and $\Omega_\Lambda$=0.7. All magnitudes quoted in the paper are in the AB system.
\section{QJ~0158-4325\, and dataset}\label{theqso}
 The quasar was detected in the Cal\'an-Tololo Quasar survey (Maza et al. 1995), therefore called CTQ~414, and confirmed to be a lensed quasar (at z=1.29) by  Morgan et al. (1999). The two images of the quasar are separated by 1.22\arcsec. A galaxy overdensity was detected along the line-of-sight to the quasar (Faure et al. 2004), suggesting the presence of a galaxy group. \\
 There  remains in the literature a discrepancy of $\sim$0.8\arcsec\, between the absolute declination of image A (see label in Fig.~\ref{deconv}) by Morgan et al (1999) and that provided in the CASTLES database (Mun\~oz et al 1998). In order to elucidate this offset, we have matched the USNO-B1 stellar catalogue to the FORS R-band  images of the lens (presented in Faure et al. 2004): the RMS values are 0.07\arcsec\, and 0.06\arcsec\, in RA and DEC  respectively. We have then derived the absolute astrometry of image A: $\alpha_{J2000}=$01$^{h}$58$^{m}$41.43$^{s}$ and $\delta_{J2000}=$-43$^{o}$ 25\arcmin 3.5\arcsec. \\
Recently Morgan et al. (2008) have  published the continuum light curves of the quasar images, monitored during four seasons at the Apache Point Observatory (SMARTS) and at ESO/La Silla (Euler Swiss Telescope). However, they were not able to derive a reliable time delay, as microlensing events overwhelmed the intrinsic variability, and their best guess, for a realistic mass model (image A leading) is: $\Delta t_{AB}\sim$-20 to -10~days. The system is still under photometric  monitoring.\\
We have retrieved NICMOS-2 (Near Infrared Camera and Multi-Object Spectrometer)  F160W  images of QJ~0158-4325\, from the HST archival data related to a large public survey of gravitational lenses (PI: Falco, CASTLES\footnote{http://cfa-www.harvard.edu/castles}). \\
From the VLT archive, we have retrieved a set of four long-slit spectra centered on the quasar images and on the lensing galaxy, obtained with FORS2 (PI: Rix).
Each spectrum has an exposure time of 1300~s. The spectra were taken through an 0.7\arcsec slit, under a mean seeing of 1.28\arcsec. The resolution is 4.86~\AA\,pix$^{-1}$, from 5500~\AA\, to 11000~\AA.
The spectra have been reduced following Eigenbrod et al. (2006). It is not possible to disentangle the quasar light from the light of the lensing galaxy through a direct analysis of the spectra. However, the spectra are suitable for spectral deconvolution. \\
\section{Deconvolution}\label{deconvsec}
\subsection{Spectral analysis and flux ratio} \label{decspeceg}
In order to measure the redshift of the lensing galaxy  we have applied the spectral version of the MCS deconvolution algorithm (Magain, Courbin \& Sohy 1998, Courbin 1999) to separate the  lensing galaxy from the  much brighter quasar images in the FORS2 spectroscopic dataset. The long-slit FORS2 data do not sample any star. To circumvent this difficulty, we have modified the deconvolution strategy, compared to previous studies (e.g. Eigenbrod et al. 2008): we do not use stars, but instead the two bright quasar images as point spread function (PSF) references. We then deconvolve the data considering three point sources (two for the quasar images A and B, and one for the lensing galaxy). Along the deconvolution, the software optimizes the positions and intensities of the spectra, and at the end yields the individual spectra of the three point sources. The spectra of the quasar images  display strong \ion{Mg}{II} and weak [NeV] and H$\delta$ emission lines (Fig.~\ref{Q0158_qso}). The bright \ion{Mg}{II} doublet is used to derive the redshift, through a two-line fit. Using the measured line centers and the rest wavelengths [2795.5\AA{}, 2802.7\AA{}] for the \ion{Mg}{II} doublet, we deduce a redshift z=1.294$\pm$0.008 for the quasar.  Fig.~\ref{Q0158_lens} shows the final one-dimensional spectrum of the lensing galaxy, smoothed with a 24~\AA\ box. Residuals of the quasar \ion{Mg}{II} line are negligible, assessing the efficiency of the spectral decomposition. The lensing galaxy spectrum exhibits the typical absorption lines of an elliptical galaxy at z=0.317$\pm$0.001 (based on the position of the following lines: Gband, H$\beta$, Mgb, FeII, NaD and H$\alpha$).
\begin{figure}[h!]
\begin{center}
\includegraphics[width=8.7cm]{plot_qsospec.jpg}
\caption{Spectra of the images of QJ~0158-4325. Top spectrum:  image A. Bottom spectrum:  image B. Bottom panel: ratio between the two spectra.}
\label{Q0158_qso}
\end{center}
\end{figure}

\begin{figure}[h!]
\begin{center}
\includegraphics[width=8.7cm]{lens.jpg}
\caption{Spectrum of the lensing galaxy. The total integration time is 5000~s. The template spectrum of a redshifted
elliptical galaxy at z=0.317 is shown for comparison (Kinney et al. 1996).
Atmospheric absorptions are indicated by the  label {\tt atm}.
}
\label{Q0158_lens}
\end{center}
\end{figure}
In $\S$~\ref{intro} we have listed the phenomena which can affect the observed FRs between quasar images.  Let us discuss now the FR genuinely due to the lens and the confidence with which it can be used in the lens mass model. \\
The quasar image spectra exhibit clearly  the \ion{Mg}{II} line, which is expected  to arise from a region in the quasar, (i) which is too large to be sensibly magnified by microlensing (Abajas et al. 2002, Eigenbrod et al. 2008), and (ii) with intrinsic flux variation appreciable over a time scale  of months to years (Peterson 2001). Therefore, this broad, low ionization emission line is mainly affected by galactic extinction and by the lens magnification. Another source of flux variation could be substructures associated to the lensing galaxy on the milli-arcsecond scale (such as a dark matter clump or a dwarf galaxy). In the available dataset, we have no evidence for the presence of such substructures. Therefore we assume that there is no perturbation of such scale.\\
The FR in the \ion{Mg}{II} line  is a function  of the flux measured in the emission line, $E_i$, and in the continuum, $C_i$. The ratio between images A and B spectra (Fig.~\ref{Q0158_qso}, bottom panel) exhibits two remarkable facts, (i) a different value of the FR depending on whether it is measured in the continuum or in the \ion{Mg}{II} line and (ii) a slightly negative slope.
As to the first fact, the quasar continuum is associated with the emission of an accretion disk, the projected size of which is comparable to the Einstein radii of stars in the lensing galaxy (e.g. Anguita et al 2008). Therefore, the continuum emission is prone to be magnified (or de-magnified) by individual stars in the lensing galaxy. The intrinsic variation of this region may happens to be fast (days or weeks).  As to the second fact, the slope in the continuum FR could be explained either by microlensing or by galactic extinction. \\
The continuum and emission line ratios  vary for different reasons, hence to  measure properly the FR in the emission line it is necessary to remove the contribution of the continuum. The FR in the \ion{Mg}{II} line is given by: $\frac{F_A}{F_B}$=$\frac{E_A-C_A}{E_B-C_B}$=5.52 (or $\Delta(m_B-m_A)$=1.85~[mag]). The quasar image B being closest to the lensing galaxy center, it is at the same time less magnified by the lens and more extinguished by the lensing galaxy, than image A. Hence, the value $\Delta(m_B-m_A)$=1.85~[mag] is an upper limit of the difference due to the potential of the lens. Yet, the elliptical nature of the lensing galaxy tells us that the differential galactic extinction is likely to be fairly small and that the lens magnification is indeed the dominant contributor.

\subsection{Image deconvolution and  galaxy light profile}\label{imdec}

\begin{figure*}
\begin{center}
\includegraphics[width=12cm]{figF160_2.jpg}
\caption{\label{deconv} Deconvolution of QJ~0158-4325\ images (F160W). North is to the top, East to the left. {\it a}) Original image.  {\it b}) Deconvolved image: the quasar images A and B appear as point sources, the lensing galaxy is the sum of a de Vaucouleurs profile plus the residuals which are not fitted by the light profile. The white contours trace the light distribution of the smooth objects (quasar host galaxy and flux residuals of the lensing galaxy). (c) de Vaucouleurs luminosity profile of the lensing galaxy, with a lower flux cut than in image (b), in order to highlight its orientation and ellipticity. }
\end{center}
\end{figure*}

Moreover, we have applied the MCS deconvolution code to the  NICMOS/F160W images. A technique to build the PSF when no star is available in the field is the iterative method described in Chantry \& Magain (2007).
  As a starting point, we used {\it Tiny Tim} PSFs (Krist \& Hook 1997) already improved by the iterative method applied on another lensed system (the Cloverleaf, see Chantry \& Magain 2007) observed under similar conditions. Then we deconvolve simultaneously the four NICMOS exposures.  Doing so we obtain a good estimate of the background level, which we subtract from the initial individual exposures. The images cleaned from their background are then deconvolved simultaneously to reach a final FWHM=0.07\arcsec. The result is displayed in Fig.~\ref{deconv}. The quasar host galaxy is visible under quasar image A.\\
In addition, a fit of the lensing galaxy luminosity profile is performed during the deconvolution. A good fit is obtained with the de Vaucouleurs profile, as already mentioned in Rusin et al. (2003) and Morgan et al. (2008). We find the following parameters for the lensing galaxy light profile: PA =61$^\circ$, $\epsilon$=0.32$\pm$0.01, r$_{eff}$=0.70$\pm$0.01\arcsec. The magnitude and relative position are displayed in Table~\ref{photom}.  The value of the effective radius is in agreement with a previous study of this system by Rusin et al. (2003, r$_{eff}$=0.66$\pm$0.04\arcsec) for the lensing galaxy, using data from the HST WFPC (F814W and F555W) and the same NICMOS (F160W) observations.  In the band F160W, they found the lensing galaxy to be $\sim$0.2~mag brighter than in the present study: an explanation would be that the light of the host galaxy under the quasar image A was not removed properly, leading to an overestimation of the lensing galaxy total flux.  In Table \ref{photom},  the error bars  correspond to the standard deviations of the mean values measured in the individual deconvolved frames.

\begin{table}
\renewcommand{\arraystretch}{1.0}
\centering
\begin{center}
\caption{\label{photom} Summary of astrometric, photometric and redshift measures.}
\begin{tabular}{l l l l l l l }
\hline
\hline
            & A &B &G     \\
\hline
$\Delta \alpha$ ('') &  0 & -1.156$\pm$0.001 &  -0.780$\pm$0.001 \\%

$\Delta \delta$ ('') &  0 &-0.398$\pm$0.002 &  -0.246$\pm$0.002 \\%
\hline
z&  1.294$\pm$0.008 & 1.294$\pm$0.008 &  0.317$\pm$0.001 \\
\hline

F160W &  16.24 $\pm$0.02 & 17.02$\pm$0.02 &   16.88$\pm$0.05  \\

\hline
\end{tabular}
\end{center}
\end{table}

\section{Mass models}\label{simple}

We use the Lenstool code (Kneib et al. 1993, Jullo et al. 2007) to model the lens, where the  singular isothermal ellipsoid (SIE) is parameterized by its position, its  position angle, its ellipticity and its velocity dispersion.  During the modelling, the position, ellipticity and position angle of the lens are fixed to the values measured on the deconvolved NICMOS images (see $\S$~\ref{imdec}). The redshifts of the source and lensing galaxy are fixed to the new values measured in this paper. The only free parameter is the velocity dispersion. We find an acceptable fit ($\chi^2\sim$18) for the SIE, but the predicted FR between the quasar images is four times larger than observed (see $\S$~\ref{decspeceg}). The predicted time delay is -12.2$\pm$0.1 days. If we force the FR to be equal to the value measured in the \ion{Mg}{II} line, and in exchange let free the position angle of the galaxy or its ellipticity, we do not find any good fit ($\chi^2>>$100), showing that a single SIE cannot explain such a low FR between the quasar images. \\
Then, we model the lens with a truncated pseudo-isothermal elliptical  mass distribution (TPIEMD; Kassiola \& Kovner 1993, Kneib et al. 1996) for both the bright and dark components of the lens.  The TPIEMD has a  core radius $r_{core}$ and cut radius r$_{cut}$: we fix $r_{cut}$=$\frac{4}{3}$r$_{eff}$ (see Eliasdottir et al. 2007) and $r_{core}$=0.01\arcsec, with the aim of keeping  r$_{core} << $r$_{cut}$. By fixing r$_{cut}$ as a function of r$_{eff}$ we effectively define a constant mass to light ratio lens potential. Doing so, the number of free parameters is reduced to one: the velocity dispersion. The FR predicted  is slightly larger than the upper limit calculated from the spectra. If we force the FR to match the observed one and free the position angle or the ellipticity (within the error bars given by the deconvolution) we obtain a good fit ($\chi^2$=2.15). Using a different value for  r$_{core}$  (equal to 0.005\arcsec\, or  0.05\arcsec)  modifies slightly the time delay (respectively -14.2$\pm$0.1~days and  -14.7$\pm$0.1~ days). Results of the models are summarized in Table~\ref{modelsimple}. The error bars correspond to $\Delta \chi^2$=1. \\

\begin{table}
\renewcommand{\arraystretch}{1.0}
\centering
\caption{Parameters of  the  lens mass models.
Col. 2: $\chi^2$ of the fit.
Col. 3: Velocity dispersion (km~s$^{-1}$).
Col. 4: Time delay  in days (image A leading).
Col. 5: FR  (image A brighter).}
\label{modelsimple}
\begin{tabular}{c| c c c c c }
\hline
\hline
 & $\chi^2$&$\sigma_v$      & TD& FR  \\
\hline
SIE & 18.8  & 183.5$\pm$0.2         &-12.1$\pm$0.1 &23.4$\pm$1.3 \\
TPIEMD &3.8 & 179.9$\pm$0.2 &-14.4$\pm$0.1 &6.5$\pm$0.3\\
TPIEMD &4.7 &179.7$\pm$0.2 &-14.5$\pm$0.1 &5.52 (fixed)\\
\hline
\hline
\end{tabular}
\end{table}

\section{Conclusions}\label{dandc}
 We have measured the redshift of the lensing galaxy and improved the measurement of the quasar redshift in QJ~0158-4325. While modelling the lens, we noticed that using only the quasar image positions to constrain the mass model does not allow to discriminate a mass density profile over another: in the case of QJ~0158-4325, both a SIE and a TPIEMD appear as suitable approximations of the lensing potential. If we add the constraint of the quasar image FR (measured in the \ion{Mg}{II} line), it becomes possible to discard the SIE as a suitable approximation of the lensing potential. The lens modelled as a TPIEMD is good. The time delay inferred with the TPIEMD is $\Delta$t$_{A-B}$=-14.5$\pm$0.1 days for $H_0$=73~km~s$^{-1}$~Mpc$^{-1}$.\\
In conclusion, using the  FR to constrain the lens allows to select the most suitable galaxy profile and to measure its mass, as well as to predict the time delay with more confidence (or the Hubble constant if the time delay is known).

\begin{acknowledgements} We thanks F. Courbin for discussions and suggestions. C.F. thanks G. Letawe for giving access to the new version of the MCS software. This work started under  the support from the European Community's Sixth Framework Marie Curie Research Training Network Programme, Contract No.  MRTN-CT-2004-505183 ``ANGLES''. D.A. acknowledges travel support from ESO, CNRS and CEA at different stages of advancement of this paper. J.-P.K. acknowledges support from CNRS. The HST data used  in this paper were obtained by the ``CfA  Arizona Space Telescope  LEns Survey''  (CASTLES) collaboration (PI:  E.  Falco)
\end{acknowledgements}

redpajama_set_name: RedPajamaArXiv


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NEW WORLD - OLD GIANTS
A mere four hundred years ago, some of the great explorers of the world – history book names – came face to face with giants in old Patagonia. During the two thousand years before the Christian era, the vast lands of the Americas were inhabited by tribes of giants, much the same as those of the Middle East. As did their biblical brethren, the mighty men of America dwindled slowly away, the survivors moving ever southwards until reaching their last home, the southern tip of Argentina. It was here, as the first tentative exploration of the New World began, that Europeans encountered the few that were left.
The first of these chronicled sightings occurred in 1520, when the famous Portuguese explorer Magellan anchored his ships in the harbour of San Julian. On going ashore, he and his crew were startled to encounter a giant of a man, nearly ten feet tall and with, so they related, a voice like a bull. Enquiries soon, ascertained that he was not alone, but belonged to a tribe of giants who lived nearby.
Thoroughly intrigued, Magellan and his men captured two specimens, intending to take them back to Europe. He shipped them aboard and set sail, but they died before the return journey was halfway completed. Sir Francis Drake, who passed through San Julian in 1578, mentions that he saw two men who stood nine feet tall, and in the years that followed similar reports were made by adventurers whose names may not be quite so familiar. Pedro Sarmiento, Tome Hernandez, Anthony Knyvet and Sebald de Weert all claim to have laid eyes on the South American giants. In 1615, two more travellers, Jacob le Maire and Wilhelm Schouten, recorded the fact that they had discovered a pair of human skeletons, each nine feet in length.
By 1700, the giants seemed to have moved away from San Julian, and the next official record places them at Valdivia, Chile. In 1712, the Spanish authorities there filed repeated reports of a race of giants living in the wild interior, not many miles from the town. The last sighting seems to have taken place in 1764, when Commodore Byron, grandfather of famous poet, saw them at Cabo Virgines.
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Suffolk County Executive Steve Bellone today announced the launch of a new website, hikebikesuffolk.com, for the public to provide input on the County's Hike and Bike Master Plan. The web tool is an online map that allows users to make specific comments or recommend routes or improvements to Suffolk County's network of hiking and biking trails. Comments and recommendations will be used to create the County's Hike and Bike Master Plan.
The online tool is an interactive crowdsourcing map specially designed to gather input and data from the people who know our bike lanes and trails the best – the hikers, runners, long-distance cyclists, casual bike-riders, parents, nature enthusiasts and everyday residents who use these resources year-round. Using this new public input tool, residents can 'drop a pin' to comment on a specific location, or 'draw a path' to connect two points they would like to see better connected.
Using funding from New York Metropolitan Transportation Council obtained by Suffolk County's Department of Economic Development & Planning, the Hike and Bike Master Plan will identify the existing regional hike-bike network, identify gaps in that network, and develop an implementation plan to prioritize and fill those gaps. This plan will provide Suffolk County with a comprehensive and coordinated vision for a connected network of hiking and biking trails County-wide, facilitating transportation, recreation, tourism, and economic development.
The goal is to create a trail that promotes local tourism throughout Suffolk County and connects residents and visitors alike to our beaches, parks, education centers, downtowns and more. Multi-use trails promote healthy lifestyles, improve recreation options, and support the island's tourist economy.
The creation of the master plan includes strong community engagement by incorporating broad public input and targeted stakeholder outreach. A completed master plan and suite of recommendations are expected by the end of 2019. The County will be collecting input on the plan through May 19.
This project complements recent efforts to extend the Empire State Trail, a 750-mile trail from New York City to the Canadian border, through and across Long Island via the Empire State Trail Extension. Suffolk County's local hike-bike master plan will extend the reach of the Empire State Trail throughout Suffolk County.
Additionally, the Suffolk County Department of Economic Development will be on hand at a number of events this month and next, to discuss the hike and bike plan. These events include Earthstock at Stony Brook University on April 19th, Seatuck's Eco-Carnival at The Seatuck Environmental Association in Islip on April 27 and the Huntington Tulip Festival at Heckscher Park on May 5.