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Antioxidant and Anti-inflammatory
Punicic Acid
Punicic Acid is the main fatty acid found in Pomegranate Seed Oil and found in Pomegranates, it may contribute to many of the health benefits associated with Pomegranates.
Our evidence-based analysis on punicic acid features 15 unique references to scientific papers.
All content reviewed by the Examine.com Team. Published: Jul 12, 2013
Fat-burner
Pomegranate Seed Oil
Pomegranates (the fruit the oil comes from), Punicalagins (polyphenols in pomegranates)
How to Take Punicic Acid
Studies that use pomegranate seed oil use 400mg of a 72% punicic acid seed oil. While this appears to be in the bioactive range of punicic acid, it is not known if this is an optimal dosage or not.
The Human Effect Matrix looks at human studies (it excludes animal and in vitro studies) to tell you what effects punicic acid has on your body, and how strong these effects are.
HDL-C
Although there are possible increases in HDL-C with punicic acid, this has not been noted all the time and may be unreliable
A possible slight reduction in triglycerides has been noted with pomegranate oil, but this appears to be unreliable
Fat Mass
No significant influence on fat mass by itself
No significant influence on fasting insulin levels
No significant alterations in insulin sensitivity noted
LDL-C
- Very High See 2 studies
No significant influences on LDL-C levels
Lean Mass
No significant influence on lean mass has been noted with punicic acid supplementation
TNF-Alpha
No significant influence on serum TNF-a levels
Total Cholesterol
No significant influence on total cholesterol levels
No significant influence on weight has been noted
NOTE: The above table includes studies on Pomegranate Seed Oil as Punicic Acid is the main bioactive. Water extracts of pomegranate such as juice is gathered on the Punicalagins page
Scientific Research on Punicic Acid
1Sources and Structure
Punicic Acid is found in:
Pomegranates at 63.5% total fatty acid profile,[1] with another 14.2% possibly being isomers of Punicic Acid.[2] As pomegranates contain slightly over 1% fatty acids on a wet weight basis, 300g of fresh pomegranate confers 3g Punicic acid (estimate)
Trichosanthes kirilowii seeds, at 24.3% of the fatty acids by weight and 3g Punicic acid per 24.5g seeds[3]
Punicic acid is named after its source, Pomegranates, which have the vernacular name of Punica granatum.
1.2Structure
Punicic Acid is a conjugated linoleic acid molecule, but not one of the fatty acids referred to as supplemental CLA; typical Conjugated Linoleic Acid (CLA) supplements contain linoleic acid molecules with two double bonds in various locations; Punicic Acid contains a third double bond, is known as cis9, trans11, cis13, and is referred to as an 18:3 fatty acid rather than an 18:2 fatty acid (amount of carbons in the side chain: amount of double bonds). Structurally, it is the c9t11 Conjugated Linoleic Acid isomer with a cis double bond added on the side closer to the tail.
It is one of the main 5 18:3 conjugated linoleic acid molecules, with the others being alpha-eleostearic acid (cis9, trans11, trans13), jacaric acid (cis8,trans10,cis12), catalpic acid (9trans,11trans,13cis) and calendic acid (8trans,10trans,12cis).[4][5]
Similar to Conjugated Linoleic Acid, Punicic acid may eventually refer to a category of 18:3 conjugated linoleic acids and may not be a single molecule; the above is the standard Punicic acid molecules found in Pomegranates
2.1Serum
Ingestion of 3g Punicic acid for 28 days (via the seeds of Trichosanthes kirilowii) increases the content of Punicic acid in circulating phospholipids from negligible amounts to 0.34+/-16% of total lipids[3] and similar study design, when replicated, led to an increase from negligible to 0.47+/-0.04%.[4]
It was found in rats that Punicic acid, which is a c9t11c13 fatty acid, could be rapidly metabolized into circulating c9t11 conjugated linoleic acid,[6] similar to another 18:3 fatty acid mentioned earlier, the c9t11t13 alpha-eleostearic acid.[7] This, if replicated in humans, would mean some of the bioactivity of Punicic Acid is due to c9t11 CLA. A study designed with a 7 day adaptation period where participants were advised to not consume sources of CLA (ruminant foods) followed by 28 days punicic acid intervention (via Trichosanthes seeds) found that while the control group had CLA levels circulating from 0.05-0.06% of total fatty acids, the Punicic Acid intervention rose to 0.23+/-0.03% of total fatty acids (although Punicic acid itself was found, suggesting partial metabolism).[4] This replicated the effects found in a previous phamacokinetic study noting higher than normal CLA levels, but did not control for dietary intake.[3] It appears Punicic acid can incompletely get metabolized into c9t11 Conjugated Linoleic Acid
Punicic Acid can be metabolized into the lesser potent isomer of Conjugated Linoleic Acid known as c9t11
3Obesity and Fat Mass
3.1Fat Oxidation
Punicic acid, via the seeds of Trichosanthes kirilowii, has been shown to increase lipid peroxidation via measurements of 8-iso-PGF2α;[3] if motifs from Conjugated Linoleic Acid research are carried over (due to similar structures), this may be indicative of peroxisomal oxidation of Punicic acid and not actually indicative of lipid peroxidation.[8] Regardless of the mechanisms, 28 days of ingesting 20.8g of the seeds (12.5g fatty acids with 3g Punicic Acid) daily, relative to control (sunflower seeds), increased urinary 8-iso-PGF2α by approximately 50% without influencing C-reactive protein or IL-6.[3]
3.2Interventions
In interventions where weight is measured although not the primary goal of the research, 28 days of 3g Punicic acid shows no effects on weight reduction[3] and 800mg of Pomegranate seed oil with 72% Punicic acid content in hyperlipidemic individuals shows no benefit to weight reduction.[9]
4.1Enterocolitis and the Intestines
In a rat model of Necrotizing Enterocolitis (NES), Pomegranate Seed Oil at 1.5% of the diet was able to suppress the occurrence of NES (from 61% to 26%) and normalizing inflammatory biomarkers (TNF-α and interleukins) were measured in the ileum.[10]
5Interactions with Lipid Metabolism
5.1Triglycerides
4 weeks of Pomegranate Oil supplementation (800mg, 72% Punicic Acid) has been shown to reduce triglycerides in hyperlipidemic adults from 3.45+/-1.56mmol/L to 2.75+/-1.40mmol/L (20% decrease) without significantly affecting body weight.[9] Secondary to the lower triglycerides, a better ratio of HDL:TG was seen as HDL-C was nonsignificantly increased from baseline values.[9] These effects were replicated by the same researcher(s) 2 years later, where 45 hyperlipidemic adults had similar decreases in TGs with exactly the same magnitude and variance.[4]
A study done on healthy youth noted no influence on triglyceride levels, or any measured lipoprotein (HDL-C, LDL-C).[4]
Appears to have the ability to reduce triglycerides, but I would not put too much faith into it due to the probability of rehashed data is higher than the probability of getting the exact same standard deviations in two independent trials
6Interactions with Cancer
6.1Breast Cancer
In vitro, Punicic acid appears to have the ability to inhibit breast cancer cell proliferation at 40uM, and did so in both an estrogen responsive and estrogen non-responsive cell line.[11] In the cell lines of MDA-MB-231 and MDA-ERa7, proliferation was inhibited by 92% and 96% while apoptosis via a disrupted mitochondrial membrane potential via PKC was induced in 86% and 91% of these cell lines, respectively.[11] These effects were secondary to Punicic acid's pro-oxidative effects, as these effects were abolished by 20uM Vitamin E tocotrienol incubation.[11] Another study conducted found lower numbers (70-75% inhibition) at 50uM, and noted that the 18:3 conjugated fatty acid known as alpha-eleosteroic acid was more potent, fully inhibiting proliferation at 50uM of MDA-MB-231 and MCF-7 cell lines.[12]
Punicic acid has been demonstrated to be an anti-estrogen on ERa with an IC50 of 7.2uM and on ERb with an IC50 of 8.8uM with slight preference towards the ERa subset.[12] The IC50 values for ERa and ERb were 2.7-fold and 1.36-fold lower relative to resveratrol with similar potencies (Punicic acid being 0.0040-0.0067% as potent as 17β-estradiol on the receptor, Resveratrol being 0.0024-0.0029% as potent).[12]
Punicic acid, at low concentrations (1.8-2uM) is able to activate both of the estrogen receptors while at higher doses (101uM and 80uM for ERa and ERb) antagonized both estrogen receptors.[12] Thus Punicic acid may be a Selective Estrogen Receptor Modulator (SERM) compound.
8.1Xanthigen
Xanthigen is a brand name for fucoxanthin, a potential fat burning carotenoid from seaweed, with Pomegranate Seed Oil as a base; thus confering both the bioactivities of Punicic acid and Fucoxanthin. Fucoxanthin itself is implicated in fat loss, and human trials using Xanthigen have shown significant fat loss over time.[13] In vitro, the two molecules show some degree of synergism in pro-fat loss effects.[14]
Mechanisms of synergism, but no real estimate as to how much of fucoxanthin's benefits are enhanced by Punicic acid
^ Vroegrijk IO, et al. Pomegranate seed oil, a rich source of punicic acid, prevents diet-induced obesity and insulin resistance in mice. Food Chem Toxicol. (2011)
^ Schubert SY, Lansky EP, Neeman I. Antioxidant and eicosanoid enzyme inhibition properties of pomegranate seed oil and fermented juice flavonoids. J Ethnopharmacol. (1999)
^ a b c d e f Effect of punicic acid naturally occurring in food on lipid peroxidation in healthy young humans.
^ a b c d e Yuan G, et al. Incorporation and metabolism of punicic acid in healthy young humans. Mol Nutr Food Res. (2009)
^ Iwabuchi M, Kohno-Murase J, Imamura J. Delta 12-oleate desaturase-related enzymes associated with formation of conjugated trans-delta 11, cis-delta 13 double bonds. J Biol Chem. (2003)
^ Yuan GF, Yuan JQ, Li D. Punicic acid from Trichosanthes kirilowii seed oil is rapidly metabolized to conjugated linoleic acid in rats. J Med Food. (2009)
^ Tsuzuki T, et al. Alpha-eleostearic acid (9Z11E13E-18:3) is quickly converted to conjugated linoleic acid (9Z11E-18:2) in rats. J Nutr. (2004)
^ Iannone A, et al. Impairment of 8-iso-PGF(2ALPHA) isoprostane metabolism by dietary conjugated linoleic acid (CLA). Prostaglandins Leukot Essent Fatty Acids. (2009)
^ a b c Mirmiran P, et al. Effect of pomegranate seed oil on hyperlipidaemic subjects: a double-blind placebo-controlled clinical trial. Br J Nutr. (2010)
^ Coursodon-Boyiddle CF, et al. Pomegranate Seed Oil Reduces Intestinal Damage in a Rat Model of Necrotizing Enterocolitis. Am J Physiol Gastrointest Liver Physiol. (2012)
^ a b c Grossmann ME, et al. Punicic acid is an omega-5 fatty acid capable of inhibiting breast cancer proliferation. Int J Oncol. (2010)
^ a b c d Tran HN, et al. Pomegranate (Punica granatum) seed linolenic acid isomers: concentration-dependent modulation of estrogen receptor activity. Endocr Res. (2010)
^ Abidov M, et al. The effects of Xanthigen in the weight management of obese premenopausal women with non-alcoholic fatty liver disease and normal liver fat. Diabetes Obes Metab. (2010)
^ Lai CS, et al. Xanthigen suppresses preadipocyte differentiation and adipogenesis through down-regulation of PPARγ and C/EBPs and modulation of SIRT-1, AMPK, and FoxO pathways. J Agric Food Chem. (2012)
Asghari G, et al. Effect of pomegranate seed oil on serum TNF-α level in dyslipidemic patients. Int J Food Sci Nutr. (2012)
"Punicic Acid," Examine.com, published on 12 July 2013, last updated on 14 June 2018, https://examine.com/supplements/punicic-acid/


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HomePlayers In FocusFATI MAGIC AT EURO 2020?
FATI MAGIC AT EURO 2020?
By Ritvik Malhotra
Updated on: June 5, 2021
Ansu Fati, the Jewel of La Masia, tore the meniscus in his left knee back in November 2020. Since then he has undergone two surgeries. His recovery hadn't gone well as his knee couldn't resist the increased workload and hence, a third surgery is not ruled out. His club have missed him dearly as Spain are hoping that Fati can return to full fitness before Euro 2020.
😱 Ansu Fati trained today with the first team. He's 1⃣6⃣ years, 9⃣ months, and 2⃣1⃣ days. What were you doing at 1⃣6⃣? pic.twitter.com/g4fEJyY8Pr
— FC Barcelona (@FCBarcelona) August 21, 2019
The Spaniard's injury was a big blow for Barcelona and particularly for the 18 year old, but this was not the first one he had recieved. Back in December 2015, Fati experienced one of his worst moments yet, in a derbi barceloni, a tackle from an Espanyol player forced him to miss almost one year with a broken leg. But this only toughened him up and, once he was back, he scored a scintillating 11 goals in his first 13 games back.
A post shared by Ansu Fati (@ansufati)
A HALT IN BREAKTHROUGH YEAR
This season he had undoubtedly been one of, if not the, most important and decisive players for Barcelona. He was an undisputed starter. Scoring 5 and setting up 4 goals in 10 matches, his maturity was being displayed in every game.
👏 👏 👏 Ansu Fati, the youngest Barça goalscorer in #LaLigaSantander 🙌🔥🎉🤩 pic.twitter.com/KmCxSvpPSH
None of Barca's attackers or wingers, excluding Messi, understand spaces like him. He elevated their ceiling and made them much better.
Ansu's career has been short up until this point, however it has gone at a lightning speed. He has been breaking numerous records since, be it domestically, internationally, with club or with his national side, being a starter in both XIs. And he has been a starter because of his maturity, intelligence, quality and ground breaking potential and not because of the different absences.
A post shared by FC Barcelona (@fcbarcelona)
Now, when nothing and no one seemed to stop him, his precocious talent suffered a major setback. These are obviously the moments of uncertainty and having patience. How he recovers from this injury would be a test to his physique but, especially, to his mental strength. And Fati has plenty of that.
A POTENTIAL RETURN AT EUROS?
The Barcelona young gun admitted that it's a dream of his to represent his national side in the European Championship although that dream can be cut short. Barcelona would want him to be 100% fit for next year's campaign. They would want him to focus on the next 15 brilliant years ahead in his career rather than focusing on getting fit in the next 15 days.
Although there is no fixed date for Fati's return, him being a part of Luis Enrique's squad would give their chances of winning this summer's European Championship a real boost.
WHAT ANSU HAD TO SAY
After winning the NXGN 2021 award, Ansu Fati talked about his dream of playing at Euro 2020 and recovering from his injury.
"I hope can be [at Euro 2020], but first I have to recover from the injury,"
"I don't know what will happen in the future, but it is a dream for any player to be able to play a European Championship."
"I don't set goals, but I do try to improve day by day, growing as a player, and as a person."
( Image Courtesy – Marca official/website )
On his official Instagram account, Fati wrote in a post
"A few years ago I had a serious injury, a fractured tibia and fibula, and I couldn't play for almost a year."
"There were many days of suffering and pain, but also a lot of learning. It helped me to appreciate the little details."
"With my family and all the professionals who helped me at that time, I promised myself to keep going and work harder than ever to get back to doing what I love the most."
"Unfortunately, now I have to live through a similar situation, which I will face with the same mentality."
"I want to thank all those people who follow me and support me on a daily basis. Football is my life and no matter how many obstacles there are, I will always have the illusion of continuing to fight for my dreams."
These comments prove his maturity, mental strength and his exceptional passion for the game. But these comments also shrink the chances of Ansu Fati making it into Spain's squad for the Euro 2020.
Ritvik Malhotra
Jordi Alba's successor
Players In Focus Aditya Kochhar -
The 40 Million clause!
Explainer Vatsal Gupta -
Revenge on Barca's mind
News Arnold Lewis -
Another underrated wonderkid
Left flank wizard
The Underrated Defender
Best from Ecuador
Prodigy from Belgium
A complete number 9

redpajama_set_name: RedPajamaCommonCrawl


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Dead Hockey Hulks' Brains Contain Addiction Clue
By Jed Bickman 09/07/11
The brains of recently-deceased NHL "enforcers" show a link between repeated beatings to the head and fatal addiction and depression.
Bob Probert had 246 fights on the ice. Photo via
This summer saw the tragic early deaths of three National Hockey League "enforcers": Derek Boogaard, Rick Rypien and Wade Belak. Their role was to dish out—and take—big hits on the ice. Boogaard, who played for the New York Rangers, died of a fatal combination of painkillers and alcohol, both of which were addictive problems for him. His brain went to a neurosurgeon at Boston University, Robert Cantu, who has studied the brains of other athletes who took repeated beatings in the head. Although the results from Boogaard's brain aren't ready, Cantu has found evidence of chronic traumatic encephalopathy (CTE) in almost all his deceased subjects who suffered from addiction, depression and anxiety, including Bob Probert, who was rated the best enforcer in hockey history in 2007. CTE is a degenerative brain disease caused by blunt impacts to the head and—because it affects the relevant areas of the brain—it can cause addiction and depression. "Anytime I hear of an athlete who has had a lot of head trauma who commits suicide, I am immediately concerned that chronic traumatic encephalopathy may have played a role," Cantu said. CTE is a growing concern in both the NHL and the NFL. The NFL announced in 2009 that it would collaborate with Cantu's program at the Boston University School of Medicine. Since then, another researcher at BU, Ann McKee, has found CTE in all eleven autopsies of NFL players that she has performed: "I have only seen this unique pattern of change with this severity in individuals with a history of repetitive head trauma."
Wade Belak
Jed Bickman
Jed Bickman is a journalist and copywriter living in the greater New York City area. He is the associate editor at The New Press. You can find him on Linkedin or follow him on Twitter.


Nissan Genuine Parts & Accessories are specifically designed for your Nissan vehicle, ensuring perfect fit, reliability, durability and security, with consistent high performance in all conditions. We regularly add new products to each range, so make sure to check back for the latest in quality products. Our most recent catalogue includes accessories for the Nissan Juke, and we provide products to fit the Navara, Qashqai, LEAF, X-Trail, and many other models.
We also stock a selection of Nissan accessories to fully personalise your car – choose some new alloys, a luggage rack or bicycle carrier, or chromed covers and fixtures to add custom style to your Nissan vehicle.
Nissan recommends its dealer network and their certified Nissan technicians to use Nissan Genuine replacement parts to maintain & repair your Nissan vehicle, we'll ensure that each part is covered by our guarantee – we'll protect your vehicle by ensuring a free replacement or repair of any defective part or component, performed by one of our trained technicians. The guarantee is valid for three years if fitted before you take delivery of the vehicle, and for one year if the accessory is added during your ownership.
Fitting costs for accessories vary between our Authorised Nissan dealers, and you should always check with your local dealership for their current fitting prices. The prices on this website are provided for guidance only, and do not include any painting costs where applicable. All prices shown include VAT, calculated at 20%.
In the case of alloy wheels, new tyres may be required. Any prices quoted do not include the cost of tyres.
Certain accessories may not be compatible with other accessories, or with standard vehicle specifications and equipment.


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Top Track 100 FAST TRACK
Spun out of Goldman Sachs in 2007 by chief executive Addy Loudiadis, 57, this London firm manages more than £50bn of assets, insuring the annuity pension schemes of clients such as Asda, the Royal Mail and British Airways. In 2017, Goldman Sachs sold its stake to a consortium of investors in a deal that valued the group at £2bn. It has donated to a Covid-19 support fund that is raising up to £100m for UK charities. It has been ranked on a "new business" profit measure of £958m in 2019, when gross written premiums were £16.6bn.
Company Rothesay Life
Activity Bulk annuity insurer
Location Central London
Sales £m 958
Profit £m 730
Year end Dec 19
Principal shareholders Blackstone (36%), GIC (36%), MassMutual (26%), management & staff (3%)
Staff 252
Website www.rothesaylife.co.uk
* Supplied by company † Annualised figure **Estimated


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Decker Building (Andy Warhol's Silver Factory)
Constructed in 1892 for the Decker Brothers piano company architect and radical anarchist John H. Edelmann, this building has been home to numerous companies. It's most famous tenant, however, was Andy Warhol, who leased studio space on the sixth floor from 1968 through 1973. The studio was known as the Silver Factory and was known for cutting-age art and decadent parties. The studio is also famous for being the place where radical feminist Valerie Solanas shot Andy Warhol and art critic and curator Mario Amaya in 1968.
The Bulding in 1894
Andy Warhol's studio
Warhol being lifted into an ambulance after being shot
Front page news of the shooting
Warhol's gunshot scars
Andy Warhol was born Andrew Warhola on August 6, 1928, and grew up in a small two-room apartment. He was the youngest of his three siblings and was known for his talent for drawing and love for Hollywood movies. When he was nine years old, Warhol got his first camera and spent much of his free time taking pictures and developing them in the family's basement. His mother, Andrej Warhola died in 1942, this same year Warhol entered into high school. Before Andrej's death, she had saved money to pay for his college education.
Warhol attended the Carnegie Institute of Technology from 1945 to 1949, and graduated with a degree in Fine Arts. Warhol's original career goal was to become a commercial illustrator, and he worked on displays at Home's department store while in college. During the 1950s, Warhol rose to become a successful illustrator. In 1962, his now-famous Campbell's Soup Can series shook the art world. This led to new opportunities for Warhol, including the chance to produce paintings of cultural icons such as Marilyn Monroe, Elvis Presley, and Elizabeth Taylor.
Warhol's first major solo exhibition was held in the Decker Building in a rented studio with tin foil wrapping, silver paint, and silver balloons-decorations that led to the nickname "Silver Factory." Warhol spent much of his time in the studio, which became both a place of work and a place of inspiration. Warhol surrounded himself with a variety of artistically-oriented people that ranged from traditional artists, actors, and musicians, to socialites, drug addicts, drag queens, and radical theorists. Despite the opposition of the landlord, Warhol's factory became notorious for its raucous parties. Famous guests included Salvador Dalí and Bob Dylan. The Factory featured experimental art and music, but commercially successful bands such as the Velvet Underground among those who performed at the Factory.
In 1965, actress Edie Sedgwick became a regular at the Factory, and was often at Warhol's side. Her association with the famous artist helped launch her career. Other aspiring actresses such as Valerie Solanas, hoped Warhol could do the same for her. Solanas asked Warhol to produce her play and gave him her script. She then accused him of losing or stealing the script and demanded compensation. In response, Warhol gave Solanas a job in one of his films. Solanas then found work as a writer for Olympia Press. Her contract required that anything she wrote would become the property of her employer, something she later believed was part of a plot by Warhol to conspire with her employer and steal her work. During one of her delusional fits of rage, Solanas stole a gun, went to the Factory, and fired three shots at Warhol. The final shot wounded Warhol, after which she also shot art critic Mario Amaya. Solanas would later turn herself into the police and plead guilty, and was diagnosed with paranoid schizophrenia. Solanas served a three-year prison sentenced and had treatment in a mental hospital.
http://www.warhol.org/collection/aboutandy/ http://www.biography.com/news/andy-warhol-and-the-factory-20750995 http://www.lomography.com/magazine/226508-the-factory-andy-warhols-studio-and-hip-hangout
Inspiration of the studio and other extra information
Official Website for the Andy Warhol Museum
Background info on events that occurred in the Silver Factory
Created by Sarah Conley (Instructed by David J. Trowbridge, Marshall University) on October 8th 2015, 6:58:05 pm.
Last updated by Clio Admin on June 18th 2018, 6:40:38 pm.
Take a walk around New York's Union Square and discover the history behind some of its buildings and monuments.
New York's Union Square Walking Tour
This short walk around New York's Union Square includes stops at several monuments and landmarks and is designed to help both residents and visitors to the city. The tour includes stops at statues dedicated to Ghandi, George Washington, Lincoln, and Lafayette and also includes the former site of Tammany Hall.


What is the difference between "the leader" and "leadership"?
What is the difference between "the leader" and "leadership"? "The leader" is the historical leadership model that has led us astray so often. It focuses on the skills, attributes, and qualities of the "the leader." It tells us what each of us must do to become a leader: be more decisive, have a vision, know the answers, demonstrate charisma, and more.
There is much value here, but it causes trouble when it locks in the assumption there can only be one leader. Of course, having multiple leaders on the same task at the same time would be chaotic.
But the world is complex. Even within a hierarchy, different people can lead different things at different times, and that is the best way to create a high-performance team: let others lead, empower them, and coach them in the process.
The most effective leaders today do not just need loyal followers, as important as they may be. The complexity and pace of today's world demand leaders at every level, voices at every meeting that collaboratively challenge the way forward, and volunteers to undertake essential projects.
Why do you want to lead? Is it for the title, the money, the prestige, the power, the perquisites, or the authority? Is it to prove something to someone, a parent, friend, or someone you want to impress?
Any of these reasons will lead to disaster. People will recognize these motives. Seeing it's all about you will turn them off. Without them as loyal, committed followers, or without them as unleashed leaders dedicated to helping you achieve your collective goals, you will fail.
As Robert Greenleaf, founder of the Greenleaf Center for Servant Leadership, sagely observed decades ago, the best leaders serve. People sense that service. Then they commit. Then they follow. Then they help you lead. Leaders serve. All of which brings us to our last critical question.
Whom do you serve? If you are serving your ego, you will fail as a leader.
Leaders serve their followers and, collectively, the organization serves its multiple stakeholders: customers, employees, vendors and partners, the community, and its owners (for a nonprofit, substitute stakeholders like donors, recipients, etc.).
The days of any organization serving only shareholders, often at the expense of other stakeholders, will hopefully be over soon. The stakeholders not well served will abandon you. Leaders serve their followers and key stakeholders.
How do you answer the most important questions about your leadership?


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Apple Scales Back Orders for Its iPhones
Component suppliers that rode the iPhone's boom are now bracing for lower sales
Apple's stock is under pressure following news that the tech giant is scaling back orders for iPhones, despite selling a record number of the devices in 2015. Photo: Getty.
Eva Dou
@evadou
Jan. 5, 2016 10:03 pm ET
BEIJING—Shares of Apple Inc. extended their descent on Wednesday, amid news that the company is scaling back orders for its iPhones.
Apple's stock fell 2% to $100.70 in afternoon New York trading. Concerns about the iPhone have weighed on Apple, with its shares down 15% over the past month. The stock fell 2.5% to $102.71 on Tuesday, after Japan's Nikkei newspaper initially reported a potential cutback in phone orders.
Apple's plans to scale back sent ripples throughout the multibillion-dollar industry that supplies and builds the company's phones.
A Chinese provincial capital promised Foxconn Technology Group —which assembles iPhones—more than $12 million in subsidies to minimize layoffs at its operations there, according to a government document.


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BAE Systems wins $36 million maintenance contract for USS Cole
BAE Systems has secured a contract worth $36.6 million from the US Navy to modernise the guided-missile destroyer USS Cole.
USS Cole will undergo one year of extensive work at the company's shipyard in Norfolk, Virginia, the ship's homeport. The contract includes options that, if exercised, would bring the cumulative value to $96.7 million.
Commissioned in June 1996, the vessel is named after U.S. Marine Corps Sergeant Darrell S. Cole, who posthumously received the Medal of Honor for his actions in the Battle of Iwo Jima.
The work is expected to begin in July for a period of 12 months and will see BAE Systems workers and sub contractors dry-dock the 505-foot-long Cole and perform upgrades and repairs to the ship's hull and engineering systems that will affect nearly every space on board.
Dave Thomas, Vice President and General Manager of BAE Systems Norfolk Ship Repair, said: "Our work on board the USS Cole is important to the service life of the ship and for expanding its capability to carry out future missions. We are prepared to perform this extensive dry-docking, working with the ship's crew, the Navy, and our industry partners."
image © US DoD
If you would like to join our community and read more articles like this then please click here
The post BAE Systems wins $36 million maintenance contract for USS Cole appeared first on Defence Online.
Microsoft sign up to the Armed Forces Covenant
Lockheed Martin to supply sniper advanced targeting pod to QEAF


Showing results by narrator "Deborah Summer"
At school, Andi has trouble focusing, and at home her room is a mess. Frustrated by her differences, Andi struggles to fit in. After visiting the doctor, Andi discovers she has ADD and learns how it affects her. Andi's Antics take a new turn as Andi learns how to help her brain pay attention. This charming story will encourage children and provides an excellent resource for parents and teachers.


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Q: fogbugz: Is there a way to view the history of a case using the api I want to get all the history of a case. Is this possible through the api?

A: Execute the search command, supplying the bug ID as the query (q parameter) and asking for the events column in the results (with the cols parameter). The URL for this will look like:
http://server/api.asp?cmd=search&q=1000&cols=events&token=xxx

In the returned XML, the <case> element (there will be just one if the bug ID is valid) will have an <events> child element with <event> children containing the history; the XML format is documented in the API documentation. If you just wanted to dump the comments on a case, for example, you could enumerate the results of the XPath query /response/cases/case/events/event/s.

A: The folks at Fog Creek Software have started a fantastic "StackExchange" using, essentially, the same software as Stack Overflow. You might want to check it out.
Fogbugz Knowledge Exchange

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text:
Q: Как записать в переменную позицию нажатого элемента recyclerview? В адаптере такой код загружает картинку и обрабатывает нажатие на элемент
Recyclerview
    @Override
    public void onBindViewHolder(final ViewHolder holder, int position) {
        Book book = booksList.get(position);
         //* Загрузка обложки из интернета. Ссылки берем из ParseTask (через MainActivity)
        Picasso
                .with(holder.imgObl.getContext())
                .load(book.getUrls())
                .into(holder.imgObl);

        holder.imgObl.setOnClickListener(new View.OnClickListener() {
            @Override
            public void onClick(View view) {
//                Toast.makeText(holder.imgObl.getContext(),
//                "Пойдем читать ", Toast.LENGTH_SHORT).show();
                Intent intent = new Intent(holder.imgObl.getContext(), SliderActivity.class);
                holder.imgObl.getContext().startActivity(intent);
            }
        });

    }

Подскажите пожалуйста, как узнать позицию нажатого элемента Recyclerview и записать в переменную, доступную к использованию в методах другого класса?


text:
\section{INTRODUCTION }
\label{sec:intro}
The European Southern Observatory Faint Object Spectrograph and Camera v2 (EFOSC2) is a highly versatile, focal-reducer based, instrument, capable of
both spectroscopy and imaging at high efficiency levels. Its design is based on EFOSC (\citealt{Buzzoni}), which was developed for
the ESO 3.6m telescope at La Silla (Chile). After EFOSC was decommissioned, EFOSC2 spent a few semesters mounted at the 3.6m; then was offered at the New Technology Telescope (NTT; with a 3.58 meter primary mirror) from April 2008 until now.
 Both imaging and spectroscopy are available for EFOSC2, and in both cases it is possible to use wave plates and a Wollaston element to
perform polarimetry: imaging polarimetry and spectropolarimetry (for detail see the EFOSC2 user manual, \citealt{usermanual}).  Over the many semesters that EFOSC2 has been available, a formidable
archive of data has been built up, which includes several polarimetric observing programmes. Unfortunately, a detailed calibration of the instrumental
linear polarisation behaviour of EFOSC2 has so far not been available in the literature, which may discourage future users and affect the efficiency of their programmes.
Because of its mounting on a Nasmyth platform, EFOSC2 has high levels of wavelength dependent instrumental polarisation which depend on the direction that the telescope is
pointing (e.g. \citealt{Tinbergen}). This can be calibrated accurately, using a large set of standard star observations. The resulting polarisation model can then be used as a starting point
for future, and past, observations, which can use a much smaller set of standard star observations to tweak the model to their observing epoch, saving
valuable observing time and increasing the accuracy of calibration. In this paper we aim to provide such a calibration of EFOSC2 broadband linear imaging
polarimetry, and make the resulting Python 3\,\footnote{\tt www.python.org} codes publicly available\footnote{The codes used for this analysis are available from the authors, or alternatively available at {\tt github.com/abh13/EFOSC2$\_$Scripts}}.

\section{Instrument}
A thorough description of the EFOSC2 instrument can be found in the EFOSC2 user manual (\citealt{usermanual}), here we
summarize some of the relevant properties. To obtain polarimetric measurements, EFOSC2 has
super-achromatic half- and quarter wave plates, and Wollaston elements with 20 and 10 arcsecond
beam separations. The Wollaston element splits the light into so-called ordinary and extraordinary beams ($o$ and $e$ beams, hereafter), with orthogonal polarisation, which are recorded simultaneously by the camera. In this work, we use the Wollaston element with 20 arcsecond separation (``Woll\_Prism20'' in the ESO headers). A Wollaston mask, made of alternating open and closed strips, is used to avoid the two images (of the two beams) overlapping; it is mounted in the slit wheel. For imaging polarimetry, the Wollaston element is mounted in the grism wheel,  see the EFOSC2 user manual (\citealt{usermanual},  their figure 1) for a schematic of the instrument parts, and Figure \ref{fig:inside} for a photo of the wheels inside EFOSC2 to give the relevant scales.
In this work, the Wollaston element and the mask (``WollMask='') are mounted such that the strips are
parallel to the CCD x-axis (East-West direction: the orientation of the EFOSC2 data is such that North is up, and East to the right). We define the $o$ and $e$ beam images to be the top and bottom images, respectively.
We used a $2\times2$ binning of the CCD, which results in a effective pixel scale of 0.24 arcsecond per pixel, and a field of view of $\sim 4.1\times 4.1$ arcminutes, though the use of the Wollaston mask means that only half of the field of view (that which falls in the open strips of the mask) is recorded in each exposure.

\begin{table*}
 \centering
  \caption{Standard stars observed in the 2016 observing run. All standards were observed in B, V and R bands. Object names in italic font identify the polarised standards, the other objects are zero polarisation standard stars. The adopted Stokes $q$ and $u$ values for the polarised standards (second and third column of this table) are taken from \cite{Fossati}. We also list the uncertainties given by \cite{Fossati} on their $q,u$ measurements for these stars. For the unpolarised standards we adopt $q = u = 0$ for all three bands; see Sections \ref{sec:unpolarisedstds} and \ref{sec:polarisedstds} for a discussion.
  \label{table:obslog1}}
 \begin{tabular}{llllllll}
  \hline
Object                          & Adopted $q$ & Adopted $u$  &   Mag.     &  Exp. time  \\
                        & ($\times 100\%$) & ($\times 100\%$) &     (V)      &  (s)       \\
 \hline
{\it BD$-$12 5133}          &$B: 1.87\pm0.04$  & $-3.95\pm0.05$ &    10.4    &   1        \\
                            &$V: 1.75\pm0.04$  & $-4.00\pm0.04$  &        &                \\
                            &$R: 1.63\pm0.02$  & $-3.68\pm0.02$  &        &                \\
{\it Hilt 652 (CD$-$28 13479)} &$B: 5.70\pm0.01$ &  $-0.11\pm0.03$  &    10.8     &  1, 2  \\
                               &$V: 6.24\pm0.03$ &  $-0.18\pm0.04$  &        &             \\
                               &$R: 6.07\pm0.02$ &  $-0.18\pm0.04$  &        &             \\
{\it Vela 1 95 (Ve 6$-$23)} &$B: 7.12\pm0.05$  & $-1.66\pm0.03$     &    12.1     &   2    \\
                            &$V: 7.91\pm0.05$  & $-2.38\pm0.06$     &        &             \\
                            &$R: 7.56\pm0.06$  & $-2.32\pm0.03$    &        &             \\
\hline
WD 1344$+$106               & &                  &    15.1     &    20         \\
WD 1615$-$154                & &                &    13.4     &    4           \\
WD 1620$-$391                & &                &    11.0     &    2           \\
WD 2039$-$202                & &                &    12.4     &    2           \\
WD 2359$-$434                & &                &    13.0     &    3           \\
 \hline
\end{tabular}
\normalsize
\end{table*}

\begin{table*}
 \centering
  \caption{ Full log of unpolarised standard star observations used in this document. $q,u$ values are the measured instrumental values in the EFOSC2
  coordinate system. ``mid'' denotes the value at the middle of the polarimetric sequence of four exposures.
 \label{table:unpol}}
 \begin{tabular}{llllllllll}
  \hline
Object                                   & Filter   &   Obs. date      & Parallactic angle & $q$                        & $q$ error                & $u$                        & $u$ error \\
                                               &            &   (mid, MJD)    & (mid; degrees)    &  ($\times 100\%$)   &  ($\times 100\%$)   & ($\times 100\%$)    & ($\times 100\%$)   \\
 \hline
WD 1344$+$106                 &     $V$       &    57558.9832     &  -160.01        &  -2.40    &     0.17         & 2.66  &    0.13             \\
                                            &     $B$       &    57558.9859      &  -161.19        &   -2.68   &      0.26        & 2.10  &   0.20          \\
                                            &     $R$       &   57558.9886      &   -162.39        &  -1.75    &      0.14        & 3.39  &   0.11          \\
WD 1615$-$154                 &     $V$         &  57560.0979    &  -146.41            &  -3.07    &   0.15           & 0.96  &  0.12             \\
                                           &     $B$         &  57560.0999    &   -148.16           &  -2.95    &   0.16           & 0.59  &     0.12        \\
                                           &     $R$         &  57560.1019    &  -149.99            &  -3.29    &    0.15          &  1.94 &   0.12          \\
                                           &     $V$         &  57560.1614   &   142.14           &  3.08   &  0.16            & 1.19  &    0.13        \\
                                           &     $B$         &  57560.1634    &    140.68          &  2.40    &    0.16          & 1.22  & 0.13            \\
                                           &     $R$         &  57560.1653    &   139.30           & 3.82     &   0.16           & 0.39  & 0.13            \\
                                            &     $V$       &   57561.9884   &    -115.78          & -2.22     &   0.13           & -2.17  &  0.10           \\
                                            &     $B$       &   57561.9905   &    -115.88         &  -1.66    &     0.15         & -2.29  &   0.12          \\
                                            &     $R$       &   57561.9925   &     -115.99         &  -3.00    &  0.13            & -2.23  &  0.11           \\
                                            &     $V$      &  57562.1725    &       131.98        &  3.56    &   0.34           & -0.46  &  0.29           \\
                                            &     $B$      &   57562.1745    &      131.01         &  3.05    &   0.27           & 0.59  &  0.16           \\
                                            &     $R$      &   57562.1766   &        130.08       &  4.16    &  0.33            & -0.44  &  0.27           \\
WD 1620$-$391                  &     $V$        &  57559.0593   &      -73.86       &     1.91 &    0.07          & -2.60  &  0.05           \\
                                            &     $B$        &  57559.0612    &      -73.09      &  2.04    &   0.07           & -2.08  &   0.06          \\
                                            &     $R$       &  57559.0631    &      -72.31       &  2.07    &   0.07           & -3.07  &  0.05           \\
                                            &     $V$        &  57559.1679    &    49.13         & -3.28     &   0.07           & -0.72  &  0.05           \\
                                            &     $B$        &  57559.1698    &    50.86         &  -2.60    &  0.07            & -1.32  &  0.05           \\
                                            &     $R$       &  57559.1716    &     52.47         &  -3.74    &   0.07           & -0.79  &    0.05         \\
                                            &    $V$        &  57560.0292   &       -83.04        &  1.05    &   0.10           & -3.07  &   0.07          \\
                                            &     $B$       &  57560.0310   &     -82.51          &  1.36    &    0.10          & -2.77  &  0.08           \\
                                            &     $R$       &  57560.0328   &     -81.98          &   0.72   &     0.09         & -3.60  &  0.07           \\
WD 2039$-$202                  &    $V$        &   57559.2199  &  -113.55             &     -2.34 &    0.13          & -2.48  &   0.10          \\
                                            &    $B$        &    57559.2218 &  -113.74             & -1.55     &   0.15           & -2.45  &  0.11           \\
                                            &    $R$        &    57559.2237 &  -113.93             & -2.86     &    0.13          & -2.36  &     0.10        \\
                                            &   $V$         &    57560.2688  &  -127.13           & -3.13     &     0.13         & -1.17  &    0.10         \\
                                            &   $B$         &    57560.2707  &  -128.24           &  -2.63    &    0.15          & -1.38  &   0.11          \\
                                            &   $R$         &   57560.2726   &  -129.42           &   -3.81   &     0.13         & -0.52  &    0.10         \\
                                            &   $V$         &    57560.4149  &  112.67            & 2.35     &   0.14           &  -2.38 &   0.11          \\
                                            &   $B$         &    57560.4168  &  112.56            &   2.66   &     0.16         &  -1.60 &   0.13          \\
                                            &   $R$         &   57560.4187   &  112.46           &  2.24    &      0.15        & -3.05  &    0.11         \\
WD 2359$-$434                  &    $V$        &   57559.3374   &  -80.87            &     1.25 &    0.15          & -3.07  &   0.12          \\
                                            &    $B$        &   57559.3393   &  -80.27            &  1.44    &    0.20          & -2.62  &    0.15         \\
                                            &    $R$        &   57559.3413   &  -79.66            &  1.07    &     0.13         & -3.46  &  0.10           \\
                                            &    $V$        &   57559.4309   &  -25.40            &  2.44    &     0.14         & 2.28  &    0.11         \\
                                            &    $B$        &   57559.4329   & -23.19             &  1.14    &       0.19       & 2.47  &    0.14         \\
                                            &    $R$        &   57559.4348   & -20.90             &  2.88    &    0.12          &  2.65 &    0.09         \\
                                           &     $V$       &  57562.2912     &    -91.09             &   -0.91   &       0.98       & -4.07  &   0.53          \\
                                            &     $B$       &  57562.2931     &  -90.62               &  -0.81    &        0.97      &  -2.70 &    0.91         \\
                                            &     $R$       &  57562.2950    &   -90.15              &   0.17   &     0.46         &  -3.54 &   0.36          \\
                                            &     $V$       &  57562.3048     &   -87.68              & 0.36     &   0.28           & -3.20  &  0.25           \\
                                            &     $B$       &  57562.3068     &    -87.18             &   1.08   &    0.47          & -2.39  &  0.34           \\
                                            &     $R$       & 57562.3087     &    -86.67             &  0.09    &    0.27          & -3.90  &    0.18         \\
                                            &     $V$       &  57562.4243    &      -23.60           &   2.35   &    0.21          & 2.56  &   0.16          \\
                                            &     $B$       &  57562.4262    &     -21.35            &  1.31    &    0.25          & 3.10  &   0.21          \\
                                            &     $R$       &  57562.4282    &     -19.05            &  2.44    &     0.17         & 2.87  &   0.13          \\
 \hline
\end{tabular}
\normalsize
\end{table*}

\begin{table*}
 \centering
  \caption{ Full log of polarised standard star observations used in this document. $q,u$ values are the measured instrumental values in the EFOSC2
  coordinate system.  ``mid'' denotes the value at the middle of the polarimetric sequence of four exposures.
 \label{table:pol}}
 \begin{tabular}{llllllllll}
  \hline
Object                                   & Filter   &   Obs. date      & Parallactic angle & $q$                        & $q$ error                & $u$                        & $u$ error \\
                                               &            &   (mid, MJD)    & (mid; degrees)    &  ($\times 100\%$)   &  ($\times 100\%$)   & ($\times 100\%$)    & ($\times 100\%$)   \\
 \hline
BD$-$12 5133                      &    $V$      &  57562.2671     &    139.50            &  7.00    &     0.10         & 2.86  &  0.07           \\
                                             &    $V$      &  57562.2688     &    138.54             &  7.06    &    0.10          & 2.89  &    0.09         \\
                                             &    $B$      &  57562.2707      &   137.59              &  6.23    &    0.19          & 3.80  &   0.14          \\
                                             &    $B$      &  57562.2724      &   136.71              &  6.31    &   0.34           & 3.52  &    0.28         \\
                                             &    $R$      &  57562.2743      &   135.82              &   7.54   &     0.17         & 1.19  &   0.14          \\
                                             &    $R$      &  57562.2760      &   135.01             &  7.66    &   0.13           &  1.25 &   0.07          \\
Hilt 652                                 &    $V$      &   57562.2486      &   97.52              &   0.31   &   0.13           & 3.67  &   0.09          \\
                                             &    $V$      &   57562.2504      &   97.64              &   0.27   &    0.07          & 3.75  &    0.06         \\
                                             &    $B$      &    57562.2522     &   97.77              &  -0.56    &    0.21          & 3.67  &      0.17       \\
                                             &    $B$      &    57562.2540     &   97.89              &  -0.62    &    0.14          & 3.44  &   0.11          \\
                                             &    $R$      &    57562.2559     &  98.03               &  0.92    &   0.09           & 2.87  &    0.07         \\
                                             &    $R$      &    57562.2577     &  98.16               &  0.89    &    0.05          &  2.78 &   0.04          \\
Vela 1 95                              &    $V$   &   57558.9728     &    84.17             &   1.45   &    0.12          & 4.65  &   0.09          \\
                                             &      $B$    &   57558.9747    &     84.71             &   0.19   &    0.36          & 4.17  &   0.27          \\
                                             &      $R$    &   57558.9765    &     85.24             &  1.64    &    0.06          & 3.47  &    0.05         \\
                                             &      $V$     &   57559.9767    &    86.07              &  1.39    &    0.12          & 4.68  &    0.09         \\
                                             &      $B$     &   57559.9785   &    86.59              &  0.40    &    0.33          & 4.85  &      0.26       \\
                                             &      $R$     &   57559.9804    &   87.10              &   1.76   &    0.06          & 3.39  &   0.05          \\
                                             &      $V$     &  57561.9775    &    87.80              &   1.55   &     0.12         & 4.55  &    0.09         \\
                                             &      $B$     &   57561.9793   &     88.32             &  0.81    &    0.37          & 5.35  &     0.29        \\
                                             &      $R$     &   57561.9812   &     88.82            &   2.09   &     0.06         & 3.33  &    0.05         \\
 \hline
\end{tabular}
\normalsize
\end{table*}

\section{Calibrator selection}
\subsection{Unpolarised standards}\label{sec:unpolarisedstds}
We select a set of unpolarised standard stars (all white dwarfs, see Table \ref{table:obslog1}), which satisfy the following constraints: $V\geq11$ mag (e.g. to avoid non-linearity problems at
lower than average seeing),
airmass $\leq1.8$, covering a range of parallactic angles at our observing nights, and which have recent observational confirmation of their status as polarimetric calibrator. The selected sources
are shown in Table \ref{table:obslog1}. All sources, with exception of WD\,1344$+$106, are confirmed zero-polarisation calibrators in the thorough study of \cite{Fossati}. WD~1344$+$106
has been studied by \cite{Zejmo}, who confirm its suitability as zero polarisation calibrator. Presence of bright Moon, cloud cover and
the general paucity of faint southern-hemisphere calibrators limited the choice of sources, and the range of parallactic angles at which we could obtain measurements.

\subsection{Polarised standards}\label{sec:polarisedstds}
The selection criteria of intrinsically polarised standards  are similar to the unpolarised ones, but here we point out that the number of (relatively) faint, well-studied, polarised standard stars in the Southern
hemisphere, visible at the time of our observations, is very small. This problem was enhanced by the unlucky coincidence that most of the few suitable sources were too close to the Moon on the first two
nights, and planned observations on the last two nights were hindered by clouds. Therefore only a small sample of polarised standards could be observed (Table \ref{table:obslog1}),
with a narrow range of parallactic angle (Table \ref{table:pol}). All of these objects are listed in \cite{Fossati} with $B,V,R$ band values for $q,u$, from both FORS imaging polarimetry and
spectropolarimetry convolved over synthetic bandpasses;
note that \cite{Fossati} show some evidence that Vela 1 95 may exhibit low level polarimetric variability.  For completeness, we also list the $q,u$ values of \cite{Fossati} for our standard stars in Table \ref{table:obslog1}.
For a first order calibration of the instrument response for a Nasmyth-mounted polarimeter it is not strictly required to observe polarised standards, but they do form a valuable additional cross-check.

\section{Observations}\label{sec:obs}
All observations were obtained on the nights of 19, 20 and 22 June 2016. Observations on the nights of 23 and 24 June were impossible
due to poor weather conditions; observations in the second half of 22 June were taken through thick and variable  clouds. The nights of
19 and 20 June had some thin hazy clouds, and poor seeing conditions.  In all cases, observations used broadband $B$, $V$ and $R$ filters (ESO filters \#639, 641, 642, respectively).
We obtained no $U$ band standard star data because of the full Moon and cloud conditions, and no $i$ band data
because fringing starts to become a complication at red wavelengths.

\begin{figure}
\centerline{\includegraphics[width=8cm]{efosc_inside.eps}}
\caption{The insides of EFOSC2, mounted on the Nasmyth focus of the NTT. Light enters from the right, the camera is on the left.
In between, the two wheels containing filters and grisms can be seen, the finger points at the Wollaston element that was used
for the EFOSC2 imaging polarimetry in this paper. }
\label{fig:inside}
\end{figure}

For all our data, we use four half wave plate angles, of 0, 22.5, 45 and 67.5 degrees, taken consecutively.
The use of four angles increases polarimetric accuracy, as outlined in detail in \cite{patat}.
The CCD was read out using $2\times2$ binning, the readout mode was  the ``normal'' mode
(see EFOSC2 user manual, \citealt{usermanual}). We used
Janesick's method (Janesick 2001) to verify the gain and readnoise in this readout mode and binning, which gave a gain of 1.18 electrons per ADU
and readnoise of 11 electrons.

The acquisition of the objects was done as follows: a short exposure without mask and Wollaston element was taken, in which the target was identified, and, after centroiding, placed on
a reference pixel position. This position was determined in the daytime, using an exposure of an internal instrument lamp, illuminating the mask. This allowed us to choose
a position near the center of the CCD but sufficiently away from bad columns and bad quality pixels. We used the pixel position (in unbinned, $1\times1$,  image pixel coordinates)
of $x,y=1100,1016$.

To reduce the data, we employ a set of bias frames and a set of polarimetric flat field images. The latter were dome screen flats, taken with the polarimetry optics in the beam
(Wollaston, wave plate, mask) and the same readout parameters as the science data.  During these flatfield exposures, the wave plate was kept rotating in a continuous fashion. This largely
scrambles the polarisation-dependent sensitivity properties in the flat fields. The science data were bias-subtracted and flat fielded using standard routines in IRAF.

The fluxes of the sources in the $o$ and $e$ beam were measured using aperture photometry. The known offset between the $o$ and $e$ beam was used to fit the centroid of the stars more accurately. We used
our IRAF package {\sc appola} (originally developed by E.~Rol), the method is described in detail in \cite{Wiersema121024} and \cite{Wiersema091018}.
Aperture radii were chosen as 1.5 times the FWHM of the stellar point spread function, determined with a Gaussian fit. Note that no difference between
$o$ and $e$ beam FWHM distribution was observed at the standard star location, and so we use FWHM values that are found from a tied fit for the
two beams. To obtain Stokes  parameters $q = Q/I$ and $u = U/I$, and reliable uncertainties, from these fluxes and flux uncertainties, we use the methods in \cite{patat}, also summarised
in \cite{Wiersema091018}. The resulting $q,u$ values are tabulated in Tables 2 and 3, and shown in Figure \ref{fig:matrixmethod}.

There are some additional complications that affect
a small number of individual datasets or images.
 Some of the data shown here were taken under very poor or highly variable cloud cover, leading to (relatively) large uncertainties in the $q,u$ values (Table 1 and 2). Several
of the standard stars are very bright, and when observed under poor seeing the relatively small strip height means that
some tweaking of the sky annulus was occasionally required, to prevent the sky annulus from incorporating some pixels from the mask gaps.  Lastly, a small fraction of the data of very
bright objects occasionally show the presence of ghost images (see EFOSC2 user manual; \citealt{usermanual}), that move as a function of wave plate rotation angle. We carefully analysed each image by hand (and inspected visually) to minimise the effects on the presented analysis.

\subsection{Off-axis behaviour \label{sec:off-axis}}
The observations above were aimed at calibrating the instrumental polarisation near the centre of the CCD - at the reference pixel position, to be precise, where we located
all our science targets too (Higgins et al. in prep.). Many polarimeters show increasing instrumental polarisation away from the optical axis, usually the shape and amplitude of this pattern is a function
of wavelength, see e.g. \cite{patat} for an example of the
FORS1 polarisation pattern, or \cite{Heidt} for the pattern of the CAFOS instrument on the Calar Alto 2.2m. To calibrate this, one can use a variety of methods: {\em i)} the sky background in regions with few objects and away from bright Moon; {\em ii)} bright fieldstars in long-exposure science datasets; and {\em iii)} a dedicated observing block of, for example, an open cluster, which has several bright member stars spread over
the field of view, that by virtue of membership of this cluster suffer from broadly identical Galactic dust induced polarisation. In this document we focus our efforts
on point sources near the center of the field of view, we will investigate the off-axis behaviour in a future study.

\section{Analysis}
\subsection{Fitting a sinusoidal relation \label{sec:cosine}}
As discussed by \cite{Heidt}, the EFOSC2 instrumental polarisation appears to follow a simple cosine curve as a function of
parallactic angle, with little evidence for additional components of instrumental polarisation.
 We fit the $q,u$ of the unpolarised standards as function of parallactic angle, using a cosine function, fit independently to $q$ and $u$ to test consistency,
i.e. the function $A*\cos(2\theta - \theta_0)$. For $B$ band, this gives for $q$: $A=2.86\pm0.05, \theta_0=104.3\pm1.2$; for $u$: $A=3.07\pm0.04, \theta_0=13.5\pm0.65$.
For $R$ band, this gives for $q$: $A=3.80\pm0.05, \theta_0=85.9\pm0.7$; for $u$: $A=3.73\pm0.04, \theta_0=-2.6\pm0.6$.
For $V$ band, this gives for $q$: $A=-3.27\pm0.06, \theta_0=274.3\pm1.3$; for $u$: $A=3.32\pm0.04, \theta_0=4.5\pm0.6$.
 It is clear that the $B,V,R$ filters show polarisation curves with different amplitudes and
with a phase difference, as
expected from the properties of metallic mirrors, and as seen in other Nasmyth polarimeters (e.g. \citealt{PAOLO} and references therein).
For a given wavelength, we expect the cosine amplitude to be the same for $q$ and $u$, and for the $q$ and $u$ data to lag each other by exactly $\pi/2$ phase. We can
therefore fit $q$ and $u$ together per band, fitting only for the amplitude and one $\theta_0$ value (with a fixed $\pi/2$ phase difference between $q$ and $u$). For $B$ band this gives $A=2.97\pm0.28, \theta_0=103.8\pm0.5$. For $R$ band this gives $A=3.30\pm0.24, \theta_0=94.4\pm0.5$. For $V$ band this gives $A=3.75\pm0.21, \theta_0=86.9\pm0.4$.

The best-fitting cosine function $q,u$ values at a given parallactic angle can now be subtracted off measured $q,u$ values of science objects to
provide a crude correction for instrumental polarisation (as done in e.g. \citealt{Heidt}). However, this would not take into full account the effects of
cross-talk, which will be substantial (e.g. \citealt{Tinbergen}), particularly affecting intrinsically highly polarised sources.
A more thorough modelling of this dataset can solve for this too, and give increased accuracy, as we set out in the next section.

\subsection{A Mueller matrix approach}\label{sec:mueller}
Fitting an empirical function as in Section \ref{sec:cosine} is a data-intensive effort, requiring many data points, often impractical for
programmes with only small time allocations. Additionally, it would leave smaller instrumental effects (cross-talk) incompletely corrected.
An alternative approach that is frequently used for Nasmyth focus mounted polarimeters,  is one where all optical elements in the light path are expressed as Mueller matrices, acting  upon the Stokes vector describing the incoming light (see e.g. \citealt{Tinbergen} and
references therein). Naturally, the tertiary mirror (M3) is the most important contributor, as these are metal-coated mirrors under a large
angle, and therefore strongly polarise incoming light. We construct a train of matrices describing all key polarising components of
EFOSC2, and fit the unknown quantities (e.g. the complex index of refraction $n_c$ [defined in terms of the refractive index $n$ and the extinction coefficient $k$  as $n_c = n - i*k$], the possible angular offsets between the
detector and the celestial reference, etc.) onto the dataset described above. The coating of M3 slowly
oxidises and dust  is accumulated on the mirror surface, and we therefore expect these indices to gradually change with time and potentially change abruptly any time the mirror is recoated or washed
(e.g. \citealt{vanHarten}). The same is
true any time the instrument is subject to an important maintenance operation that can modify the angular offset of the optical components of the whole
instrument. The calibration of a Nasmyth polarimeter for relatively simple alt-azimuthal telescopes and instruments by means of suitable trains of Mueller
matrices was addressed by several authors \citep{Giro,Joos,PAOLO} while more complex instruments were also successfully modelled \citep{Selbing,Witzel}.

\begin{figure*}
\centerline{\includegraphics[width=19.5cm]{efosc2.eps}}
\caption{ The measured $q,u$ values in $B,V,R$ bands of unpolarised standards (circles) and polarised standards (triangles, stars) are shown as a function of parallactic angle (PA) in the top two windows. The solid lines show the best fitting $B,V,R$ polarimetric Mueller matrix model solutions; the dashed lines show the same solution around the polarised stars values (using shorter lines to keep the plot legible). The bottom two windows show the residuals for $q,u$ in $B,V,R$ bands. The average $V$ band residuals of the $q$ and $u$ fits are calculated to be $\sim0.06\%$, with similar values for $B,R$ bands.}
\label{fig:matrixmethod}
\end{figure*}

\begin{figure}
\includegraphics[width=\columnwidth]{mcmc_result_Vband.eps}
\caption{ Projection of the normalised probability distributions for the detector offset angle $\phi_{\rm offset}$ and multiplication factor (MF), from the MCMC analysis, for the $V$ band dataset.}
\label{fig:mcmcresult}
\end{figure}

For our calibration effort of EFOSC2 we make use of a Mueller matrix train consisting of the following component matrices, closely following the setup for the
Telescopio Nazionale Galileo (TNG) described in \cite{Giro}:
\begin{itemize}
\item{Matrix representing the incoming source light from the M2 mirror onto the M3 mirror: $[M_{M3}(0^{\circ})]$}. The purpose of this matrix is to change the sign of $U$.
\item{Rotation matrix representing the transformation from the sky coordinates reference frame into mirror coordinates frame as a function of telescope pointing direction: $[T(-\theta_{\rm pa})]$}
\item{Matrix representing the physical properties of the M3 mirror (including the value of, and dependence on wavelength of, $n$ and $k$, mentioned above) and the $45^{\circ}$ reflection due to how the mirror is mounted: $[M_{M3}(45^{\circ})]$}.
\item{Rotation matrix representing the transformation for a change in elevation of the mirror as a change in the mirror orientation with respect to the derotator focal plane: $[T(-\theta_{\rm pa})]$}
\item{Rotation matrix representing the transformation from the mirror reference frame to the reference frame of the detector: $[T(\phi_{\rm offset})]$}.
\end{itemize}
Here $\theta_{\rm pa}$ is the parallactic angle.
This leads to a Mueller matrix for the telescope represented by the following equation:
\begin{align*}
[M_T] &= [T(\phi_{\rm offset})] \times [T(-\theta_{\rm pa})] \times [M_{M3}(45^{\circ})] \\
&\times [T(-\theta_{\rm pa})] \times [M_{M3}(0^{\circ})]
\end{align*}
where $[M_T]$ is the total matrix representing the telescope and EFOSC2,  and the contributing matrices are described above.

We use the prescription of \cite{Stenflo} to numerically evaluate the matrix components describing the M3 mirror, and use the material constants as a function of wavelength for pure aluminium as
tabulated by \cite{Rakic}, to describe the aluminium coating of M3.  A single numerical multiplication factor (an efficiency factor, as it were) is used, which adjusts the effective refractive index of the aluminium mirror to account for the fact that the mirror surface is not ideal, pure, aluminium, but shows effects of oxidation and dust (and perhaps other effects that can be caught with this simple parametrisation). This simple approach is also successfully used for e.g. the PAOLO instrument (\citealt{PAOLO}).

Using the M3 physical components described above, we give as illustration the following matrices for a reflection at $0^{\circ}$
\[
[M_{M3}(0^{\circ})] =
\left[ \begin{array}{cccc} 1 & 0 & 0 & 0 \\ 0 & 1 & 0 & 0 \\ 0 & 0 & -1 & 0 \\ 0 & 0 & 0 & -1 \end{array} \right]
\]
and a reflection at $45^{\circ}$
\[
[M_{M3}(45^{\circ})] =
\left[ \begin{array}{cccc} 0.9699 & 0.0301 & 0 & 0 \\ 0.0301 & 0.9699 & 0 & 0 \\ 0 & 0 & -0.9487 & -0.1993 \\ 0 & 0 & 0.1993 & -0.9487 \end{array} \right]
\]
for $V$ band - these values are different for $B$ and $R$ bands as the material constants are wavelength dependent.

The equations for the matrix components were implemented in a Python code, in which we fit the values of the matrices onto the large and high quality set of polarised and unpolarised standard stars described above.
This allowed us to derive a very well constrained polarimetric model (Figure \ref{fig:matrixmethod}), using only a small number of free parameters. It simultaneously corrects for the instrumental polarisation and the angular offset of the detector through the entire possible range
of the parallactic angle of any observable target. The root mean square (rms) of the residuals of the best fitting model on the observed data (Figure \ref{fig:matrixmethod}) are consistent with being due to the observational errors only. The set of polarised standard stars similarly shows excellent agreement with our model (Figure \ref{fig:matrixmethod}).
To get a better understanding of any possible degeneracies and shape of confidence contours,  we run a Markov Chain Monte Carlo (MCMC) code ({\tt emcee}; \citealt{emcee}).  We use the log-likelihood function of a normal distribution as our posterior probability distribution and attempt to find the maximum-likelihood result. We use this in conjunction with the observed $q$ and $u$ values to determine the detector offset angle with respect to the mirror's reference frame (wavelength dependent) and the afore mentioned multiplication factor.  The MCMC uses 20 walkers, each with a total of 2500 steps and a burn-in period of 250 steps. Figure \ref{fig:mcmcresult} shows the projection of the probability distributions of both the offset angle and multiplication factor (MF) for $V$ band. The parameters are clearly non degenerate, and both distributions are consistent with normal, and show low levels of variance. We see similar distributions for the parameters for both the $B$ and $R$ bands and are therefore confident that our results accurately reflect the true offset angle and multiplication factor. The resulting full calibration parameter values from the MCMC analysis can be seen in Table \ref{table:mcmc_results}.

\begin{table}
\centering
\caption{Detector angle offset and multiplication factor results from the MCMC code, for the $B$, $R$ and $V$ filters. Errors quoted are $1\sigma$.}
\begin{tabular}{ccc}
    \hline
  \multicolumn{1}{p{2.0cm}}{\centering Filter}
& \multicolumn{1}{p{2.0cm}}{\centering $\phi_{\rm offset}$ ($^{\circ}$)}
& \multicolumn{1}{p{2.0cm}}{\centering Multiplication \\ factor}\\ \hline
$B$ & $-51.9\pm0.3$ & $0.95\pm0.01$ \\
$V$ & $-47.2\pm0.3$ & $0.94\pm0.01$ \\
$R$ & $-43.5\,^{+0.2}_{-0.3}$ & $0.94\pm0.01$ \\ \hline
\end{tabular}
\label{table:mcmc_results}
\end{table}

To calibrate $q,u$ observations taken with EFOSC2, one can now invert the matrix model found above to directly get the instrument-corrected $q,u$ values from the
observed values, using the parallactic angle value.
This model could in principle be extended to spectropolarimetry or to other wavelengths (filters) with small modifications or additions to the code.

\subsection{Comparison with older observations}
An instrumental polarimetry characterisation of EFOSC2, mounted on the NTT, was undertaken by \cite{Heidt} using data taken in
2008 and 2009. These authors obtained a large number of observations of zero-polarisation standards in a single broadband filter, and find that the
observed instrumental $Q,U$ values as a function of parallactic angle can be well described by a cosine function.
In principle the data from \cite{Heidt} provide a meaningful comparison with our data, but there are some complications:
 \cite{Heidt} used a Gunn $r$ filter (ESO filter \#786, decommissioned in 2009); and there were
 two rounds of NTT mirror re-coating in between the Heidt \& Nilsson observing dates and ours, on 3-7 July 2012 and
 4-12 May 2015 (M1 + M3 mirrors). In Figure \ref{fig:Rcomp} we plot our zero-polarisation standard star $R$ band data, together with the $r$ standard star observations from \cite{Heidt}, which were taken on two epochs. As is clearly
 visible, the amplitude of instrumental polarisation appears to change significantly between epochs, a small change in phase may also be present. This demonstrates that care needs to be taken when using older archival data to calibrate new data.

\begin{figure}
\begin{center}
\includegraphics[width=7cm]{plot2_R_v2.eps}
\caption{Shown in red are the zero-polarisation standard star datapoints, in instrumental coordinates, from our programme;
in grey and white are the data points from Heidt \& Nilsson (2011). The thin red line is a cosine fit to our data, to make it easier to see the difference between the data from 2016 and those from 2008 and 2009. A  significant change in amplitude can easily be seen, a small phase shift may also be present. }
\label{fig:Rcomp}
\end{center}
\end{figure}

\section{Discussion and conclusions}\label{sec:discussion}
Our analysis above shows that a calibration of EFOSC2 linear imaging polarimetry (in $B,V,R$), using a relatively simple Mueller matrix based instrument model, is possible to
a precision of $P \sim0.1\%$:  propagating the uncertainties derived from the MCMC simulations shown in Figure \ref{fig:mcmcresult} and discussed in Section \ref{sec:mueller}, gives a value of the calibration accuracy in $V$ band of $P=0.08\%$.
This level is sufficient for the majority of the most popular science applications of EFOSC2 imaging polarimetry.

There are some important caveats and recommendations to point out here:
\begin{unnumlist}
\item While the model we built works very well with our measurements, we note that we have no measurements
of Stokes $v$ $(=V/I)$; the quarter wave plate was not mounted for our observing programme, which concerned linear polarimetry only.
The M3 reflection should produce large amounts of circular polarisation as a function of parallactic angle and wavelength, as seen by e.g. PAOLO on the TNG (\citealt{PAOLO}).
Measurements of $v$, preferably quasi-simultaneously (within a few days) with $q$ and $u$, would provide a strong additional calibration constraint,
testing the accuracy of the crosstalk terms further.
\item In their analysis of the instrumental polarisation of the PAOLO instrument on the TNG telescope, \cite{PAOLO} note that
the typical timescales through which a given calibration is valid is days to weeks. In that sense it is not surprising to find  small but significantly different instrumental polarisation values from \cite{Heidt}. The timescales of change of the instrumental polarisation
could be monitored through infrequent calibration plan observations. Using our calibration as a lead, this would require only a small number of standard star observations, and would allow more reliable re-processing of past datasets.
\item The phases of the instrumental $q,u$ curves (Figure \ref{fig:matrixmethod}) are surprisingly strongly dependent on wavelength,
more so than seen in e.g. PAOLO (\citealt{PAOLO}). We only cover the $B,V,R$ filters here, future observations covering also $U$ and $i$ filters would establish
this behaviour over a wider wavelength range.
\item As can be seen in e.g. Fig \ref{fig:matrixmethod}, our observations of polarised standards are limited to a small range of
parallactic angle, and we only observed three sources. The underlying cause of this is that the number of polarised standard stars
than can be observed from the Southern hemisphere is very small, and many are too bright for a 4m class telescope. During our observing
nights the choice was therefore limited.
\item Some improvements in accuracy of individual standard star $q,u$ values are possible. Putting aside the obvious advantages of
observations in clear and lower moonlight conditions, an increase in accuracy can also be delivered by using eight wave plate angles
instead of the four we used. Using a small amount of defocussing of the telescope will allow longer exposures and will spread the light over
more pixels, allowing more counts in the source PSF without saturating the central pixel. This latter effect can be important on nights
of good seeing, considering the brightness of the standards.
\item An explicit matrix for the half wave plate could be added. This could reduce the uncertainties that come from the fact that a given set of four consecutive wave plate angle exposures, needed for a single $Q,U$ point, spans a (small) range of parallactic angle.
\end{unnumlist}

While we only considered broadband imaging polarimetry in $B, V, R$ filters, a similar strategy for narrowband and spectropolarimetry can be employed with relatively minor adjustments to our Python codes.

\begin{acknowledgements}
This calibration effort is dedicated to the memory of dr.~Peter Curran (ICRAR, Perth). We miss his insights into polarisation properties of jet sources, but above all his generous friendship. We thank the anonymous referee for their helpful report which improved this paper.
It is a pleasure to thank the observatory staff at ESO La Silla for their help in obtaining the observations in this
document, and particularly Pablo Arias for a tour of the telescope and detailed explanation of the instrument. We are very grateful to J. Heidt and K. Nilsson for
sharing their standard star measurements with us.
Based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO programme 097.D-0891(A).
KW, ABH and RLCS acknowledge funding from STFC.

\end{acknowledgements}

\bibliographystyle{pasa-mnras}

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Fra Ante Čovo (Sinj, 29. listopada 1959.) hrvatski je franjevac i teolog.

Životopis
Rodio se u Sinju, od roditelja Ivana i Luce rođ. Vučić. U rodnom gradu završio je osnovnu školu i klasičnu gimnaziju. U Makarskoj i Zagrebu pohađao je filozofsko-teološki studij. Diplomirao je 1985. god. 29. lipnja 1986. godine zaredio se u Splitu za svećenika Franjevačke provincije Presvetoga Otkupitelja. Obnašao duhovne dužnosti u Vinjanima i u Splitu, na Dobromu (župni vikar); magistar (odgojitelj) bogoslova, tajnik za formaciju i studij, promicatelj pastorala zvanja i duhovni asistent franjevačke mladeži. Sada je ravnatelj Franjevačkoga instituta za kulturu mira. Godine 1988. započeo je u Rimu na Papinskomu učilištu Antonianum (Pontificio Ateneo Antonianum) poslijediplomski studij duhovnosti. Magistrirao je 1990. godine. Doktorirao je 1993. godine disertacijom Il francescanesimo insegnato e vissuto nelle lettere circolari della provincia del SS. Redentore in Croazia dal 1735 al 1855 (Poučavano i življeno franjevaštvo u okružnim pismima provincije Presvetoga Otkupitelja u Hrvatskoj od 1735. do 1855.), čime je stekao akademski naslov doktora teologije sa specijalizacijom u duhovnosti.

Karijera
Na Franjevačkoj visokoj bogosloviji u Makarskoj predavao od 1993. godine. U Splitu predaje od 1999. na Katoličkomu bogoslovnom fakultetu kao vanjski suradnik. Od 2005. je suradničkog zvanja višeg asistenta, a u znanstveno-nastavno zvanje izabran je docenta 2006. godine. Svoju nastavnu djelatnost završio je 2010. godine. Obnašao je dužnost tajnika Franjevačke visoke bogoslovije, a zatim je bio prodekan za nastavu (2007. – 2009.). Bio je fakultetskih povjerenstava i sveučilišnoga povjerenstva. Bio je i član Uredničkoga vijeća časopisa Služba Božja. Predavao na domaćim i međunarodnim znanstvenim skupovima, predstavljao knjige, recenzirao knjige i članke za znanstvene časopise i zbornike znanstvenih skupova. Članke objavio u Službi Božjoj, Crkvi u svijetu, Počecima i dr.
Od 2012. - 2019. godine bio je gvardijan samostana sv. Marije u Makarskoj, a od 2019. godine vrši službe gvardijana samostana u Sinju i upravitelja Gospina svetišta u istom mjestu. Dana 22. srpnja 2022., predao je službu gvardijana samostana u Sinju i upravitelja Gospina svetišta u istom mjestu svom nasljedniku fra Marinku Vukmanu, budući da su članovi Uprave Franjevačke provincije Presvetog Otkupitelja na Kapitulskom kongresu održanom u samostanu Gospe od Zdravlja u Splitu od 6. - 9. VI. 2022., donijeli odluku o razrješenju službe gvardijana samostana i upravitelja Svetišta zbog isteka mandata za službu gvardijana. Naime, zakonodavstvo Franjevačkoga reda, nalaže kako služba gvardijana samostana ne može trajati više od tri mandata ( svaki mandat traje po tri godine). Kao gvardijan upravljao je samostanom u Makarskoj sedam godina, a samostanom u Sinju tri godine.
Istodobno, predloženo je njegovo imenovanje župnikom Župe sv. Filipa i Jakova u Potravlje nadomak Sinja te je sukladno prijedlogu Provincije, splitsko-makarski nadbiskup mons. dr. Dražen Kutleša, 21. srpnja 2022. objavio dekret o imenovanju župnikom spomenute Župe.

Izvori

Životopisi, Sinj
Hrvatski franjevci
Hrvatski katolički svećenici
Hrvatski rimokatolički teolozi

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