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Dog Friendly Cottages in the Peak District
The Peak District is famous for its fantastic walks and dramatic scenery. Dovedale offers gentle valley walking with lovely views all along the length of the river, whilst for the more serious walker, the Pennine Way starts its long trek north at Edale. The region is also studded with stately homes, historic houses and friendly country pubs, many of which welcome dogs!
Please scroll down the page for a list of dog friendly cottages in the Peak District.
Harthill Hall – Henry's Haunt
Alport, nr. Bakewell, Derbyshire.
Sleeps 2 – 16. In a beautiful Peak District setting, these superb cottages have been created from an ancient cluster of listed buildings and enjoy shared use of an indoor swimming pool. Follow the link below to view other properties at this location. Cottage Code: RXX8.
Liberty House
Ashbourne, Peak District.
Sleeps 4. In the thriving market town of Ashbourne, the gateway to the Peak District, is the delightful and unique Grade II listed cottage of Liberty House – the perfect choice for those looking to explore the Peak District. Cottage Code: 998842.
Jasmine Cottage
Duffield, Peak District & Derbyshire Dales.
Sleeps 6. Nestled within the upmarket village of Duffield, surrounded by the breath-taking Derbyshire countryside is Jasmine cottage, a characterful dwelling boasting original features that have been sympathetically restored. Cottage Code: 1002550.
Fire Brigade Barn
Tissington, Peak District.
Sleeps 2. This former hay barn has been stunningly converted and restored into this one bedroom cottage in the beautiful chocolate-box village of Tissington in the Peak District National Park. Cottage Code: 932417.
Orchard View
Parwich near Ashbourne, Peak District.
Sleeps 9. Orchard View is a Grade II listed semi-detached farmhouse in the village of Parwich. Located just a few minutes' walk from the village's traditional pub and a short drive from 'The Gateway to Dovedale' the market town of Ashbourne. Traditional features such as old beams and fireplaces combine with modern comforts making this the ideal base for a holiday exploring the Peaks. Cottage Code: 2244.
Bentley's Barn
Press, nr. Matlock, Derbyshire.
Sleeps 4. Meticulously renovated, this detached single-storey barn conversion sits on the edge of the small village of Press, just a short drive from the attractive market town of Matlock. With a thoughtfully designed open-plan interior, outside there is a private hot tub. Cottage Code: UK4087.
The Barn at Grislow Field
Baslow nr. Bakewell, Derbyshire.
Sleeps 4. Found at the end of a rough track, The Barn at Grislow Field is surrounded by spectacular Peak District countryside and offers panoramic views in all directions. Set on a working farm, there are walks from the door. Cottage Code: CC412116.
Tythe Barn
Grindleford, Hope Valley, Derbyshire.
Sleeps 8. Built to take full advantage of the stunning Peak District scenery, this beautiful detached former barn has been carefully converted to provide luxurious and well-appointed holiday accommodation. Nearby is the famous 1665 plague village of Eyam. Cottage Code: RHH8.
Primrose Cottage
Diseworth, nr. Derby, Derbyshire.
Sleeps 4. Dating from around the 17th century, this chocolate box thatched cottage sits within landscaped gardens, complete with summerhouse. Inside, it has been thoughtfully decorated and features an open fire and spiral staircase. Cottage Code: UK13017.
Dale House Farm Cottage
Monyash, nr. Bakewell, Derbyshire.
Sleeps 2. Offering excellent riding and walking from the door, this characterful barn conversion provides stabling facilities for guests who wish to bring their own horse on holiday. Dating from the 1640s, it boasts a wealth of period features including exposed beams. Cottage Code: W7764.
Abacus House
Hackney nr. Matlock, Derbyshire.
Sleeps 4. This former village school boasts a very high specification, blending modern stylish features with traditional quirky twists, such as its open grate arts and crafts fireplace. Guests can enjoy excellent walks from the doorstep. Cottage Code: CC418041.


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Emmes Reports Record Growth in 2016
Download Press Release Go back to News
Emmes
The Emmes Corporation today announced the highest revenues in its 40‐year history along with significant growth in its employee count. Revenues surpassed $90 million in 2016, and it employed 567 employees in its U.S. and international offices.
This is also the first time that Emmes has appeared on the Washington Business Journal's top company lists. Emmes was the eighth largest women‐owned business in the Washington metropolitan area, according to the 2016 ranking. It was also included as one of the Washington
Business Journal's Top 100 private companies in September, with recognition in a related article about the record number of new companies on the list.
"It's an honor to be recognized as a top company in the Washington area," noted Dr. Anne Lindblad, president and chief executive officer of Emmes. "Our growth reflects a commitment to building client relationships founded on collaboration and trust. As a result, we're continuing to recruit scientists, statisticians and support staff, and this means even more opportunities for personal and professional development."
Last year, Emmes was chosen as one of the best places to work in the greater Washington area. The Washington Post's prestigious Top Workplaces list recognized organizations with the highest engagement ratings from their employees in a survey conducted by Workplace Dynamics. Emmes was one of only three biotechnology organizations on the list. The company also received a Workplace Seal of Approval from the Alliance for Workplace Excellence (AWE) for the second consecutive year.
"What we do at Emmes is support clinical trials and public health research for clients in government, corporate and non‐profit sectors," Lindblad said. "Our work and our culture attract people who think about their work in the context of preventing disease and creating more effective treatment options. The recognition we've received this past year is the result of a great team of employees."
About Emmes
We collaborate with our clients to produce valued, trusted scientific research. Our team members at Emmes are passionate about making a difference in the quality of human health, and we have supported more than a thousand studies across a diverse range of diseases since our formation in 1977. Our research is contributing to a healthier world. For more information, visit the Emmes website at www.emmes.com.

redpajama_set_name: RedPajamaCommonCrawl


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Inženjer zvuka ili audio inženjer (, ) tehničko je zanimanje. Pokriva područje tonske tehnike, studijskog i tonskog snimanja, tehnike snimanja (digitalno/analogno), obrade signala, akustike i računarske produkcije.

Tonski snimatelj, mikser zvuka i tehničar za zvučne efekte blisko su povezana zanimanja. Čine deo snimateljskog tima. Svima je zajedničko to što snimaju zvuk za sve vrste televizijskih i radijskih emisija, kao i snimanje tona za film ili snimanje muzičkog materijala.

Izvori

Spoljašnje veze
 Audio engineering formulas and calculators
 Audio Engineering Articles, Tutorials and Interviews
 Online tečaj zvučnog inženjeringa  pod licencom Krijejtiv komons
 Universität der Künste in Berlin Studium zum Tonmeister und Sound Engineer
 Institut für Elektronische Musik und Akustik KU Graz

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NEW Free Kashi Cereal. Kashi Coupons and Samples 2013.
Kashi Coupon: From the Kashi homepage, click "join the discussion." Once registered you'll get a coupon for cereal or snacks by email. You'll also get coupons by email each month when you join their newsletter. In the grocery stores, look for instore coupons for Kashi frozen foods. Right now there is a tablet with four different coupons, including $1 off (2) Kashi frozen meals.
Money Back Guarantee: If you buy a Kashi cereal and did not care for it, they'll send you a coupon for a different variety free. It's called their Smile Guarantee.
Expired: Kashi is offering a free sample of their GO Lean Crunch cereal. If you're not familar with Kashi and their products, I've been using them for a few years and they taste really good and are healthy. If you give this a try you'll be surprised.


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Elisabeth Sophie of Brandenburg (5 April 1674 – 22 November 1748), was a Duchess consort of Courland by marriage to Duke Frederick Casimir Kettler of Courland, a Margravine consort of Brandenburg-Bayreuth by marriage to Christian Ernst, Margrave of Brandenburg-Bayreuth, and a Duchess consort of Saxe-Meiningen by marriage to Ernst Ludwig I, Duke of Saxe-Meiningen. She was joint regent in Courland during the minority of her son Frederick William, Duke of Courland from 1698 until 1701.

Biography

Elisabeth Sophie was born to Frederick William I, Elector of Brandenburg and Sophia Dorothea of Schleswig-Holstein-Sonderburg-Glücksburg.

Courland
She married (29 April 1691) her cousin, Duke Frederick Casimir Kettler of Courland (1650–1698). The marriage was arranged as an alliance between the two families; in 1703 her brother Albert Frederick was to marry her first husband's daughter, Mary Dorothea.

When her husband died in 1698, Elisabeth Sophie became joint guardian-regent along with her former brother-in-law Ferdinand. In January 1701, Elisabeth Sophie left Courland, her son and stepdaughter for her brother's court in Berlin. In 1703, she was formally deprived of the custody of her son and the regency. She was later given a Russian allowance from Anna of Russia.

Brandenburg-Bayreuth
She married Christian Ernst, Margrave of Brandenburg-Bayreuth (6 August 1644 – 20 May 1712) on 30 March 1703 in Potsdam. She is said to have dominated him completely and directed his policy in a pro-Prussian direction. He gave her the palace Markgräfliches Schloss Erlangen, which was named after her. She was described as proud and a great lover of pomp and ceremony. Her expenses had a bad effect on the finances of the state.

Saxe-Meiningen
She married on 3 June 1714 on Schloss Ehrenburg to Ernst Ludwig I, Duke of Saxe-Meiningen (1672–1724).

Issue
 Frederick William Kettler, Duke of Courland (19 July 1692 – 21 January 1711).
 Leopold Charles Kettler (14 December 1693 – 21 July 1697).

Ancestry

See also
 Bibliography of Russian history (1613–1917)

References

1674 births
1748 deaths
17th-century Latvian people
17th-century women rulers
Duchesses of Courland
Margravines of Brandenburg-Bayreuth
Duchesses of Saxe-Meiningen
18th-century women rulers
Daughters of monarchs
Remarried royal consorts


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Jackie Earle Haley Can't Save This New 'Nightmare'
Eric Bourse
Wes Craven's 1984 film "A Nightmare on Elm Street" is considered a classic by horror fans. The movie revived the stale slasher genre in the 1980s by featuring a psychopath wearing gloves with five long steel blades, played by the eccentric Robert Englund, who could enter teenagers' dreams and kill them.
Fast forward to 2010, first-time feature director Samuel Bayer's remake of the beloved film is released into theaters starring Jackie Earle Haley ("Watchmen," 2009) as the dream demon, Freddy Krueger.
The film is produced by Michael Bay, who is responsible for other lackluster horror remakes such as "Friday the 13th" (2009) and 2003's "The Texas Chainsaw Massacre."
The script by Wesley Strick ("Doom," 2005) and Eric Heisserer doesn't stray too far from the original- teenagers struggle to stay awake to avoid being viciously killed by Krueger in their dreams. The biggest aspect of the original that has been lost in the remake is the most important, the horror.
The remake still contains the infamous death scenes from the original, but aren't even close in achieving the same feelings of suspense. The biggest example of this is the updated version of the iconic bedroom scene in which Krueger appears to be pushing against a wall over an unsuspecting teenager. It's a shame that the scene from the 1984 film, in which Englund is pressing through a wall made from spandex, looks much more convincing than the 2010 CGI version.
Another example from the original that has been watered down is the bathtub scene in which Krueger's claw is emerging from the soapy waters and slowly reaching the sleeping protagonists face then retreats when she wakes up. The new version has Krueger's claw coming out of the water and in a couple of seconds quickly retreats. The new scene looks more comical then the dread inducing scene from the original.
Another aspect missing from the original movie and the sequels (especially the sequels) is the surreal imagery from the nightmare scenes. The surrealism in the remake's nightmare sequences is minimal to nonexistent.
With today's technology, the writers could have come up with much more unique and frightening scenes. Instead, the film uses the same settings with the same situations too often. When there is no limit to what can happen in dreams, or nightmares for that matter, how could the writers run out of ideas?
Not all is bad in "Elm Street," however. The acting is actually better than the original, which isn't saying much. Rooney Mara ("Youth in Revolt," 2009) and Kyle Gallner ("Jennifer's Body," 2009) portray teenagers Nancy Holbrook and Quentin O'Grady, respectively. The two teens are racing to find a way to stop Krueger as they struggle to stay awake.
The standout performance in the film is clearly by Haley as "Elm Street's" villain. His performance is different from Englund's interpretation but is equally effective in creeping out the audience.
Krueger's past in the remake has been changed to a pedophile that used to molest the main characters when they were in pre-school. The new Freddy is much more sinister in this respect because he is a sexual deviant and this results in some truly creepy scenes with Holbrook.
Overall, the remake of "A Nightmare on Elm Street" is a disappointment. Similar to the other Bay remakes, the film is uninspired but destined to be a cash grab at the box office. Fans of the 1984 film will be reminded why they love the original series so much in the first place. Those who have never seen the original might become frightened by the film's many jump scenes but surely won't have any trouble falling asleep that night.
"A Nightmare on Elm Street" runs at 95 minutes and is rated R for strong violence and language.
My rating: 1 and 1/2 Stars out of 5.
Eric Bourse, Newsroom Manager
Eric Bourse was born and raised in Hollywood, California. This is Bourse's fifth year as a member of El Vaquero and has served as writer, editor-in-chief,...
Richard Kontas, Production Assistant
Production Manager; Former Editor-in-Chief and Action Sports Photographer.
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Getting Drunk in Colombia
Alcohol is known to be consumed by various people in various places over time. They consume alcohol for a variety of reasons: to relax, to excite, to loosen the tongue, to socialize, to celebrate, to show off, to live an addiction, to get drunk, etc. Moderate consumption of alcohol is socially acceptable and maybe even considered as healthy. But excessive consumption of alcohol will result in intoxicated behavior, which can be foolish and even dangerous.
Why do people consume alcohol? Some people will tell you that they do so in order to get drunk. This is obviously a controversial reason to consume alcohol. In the TGI-EGM Colombia study, which has survey data from 12,609 persons between the ages of 12 to 69 interviewed during 2003, 7.8% of the survey respondents said that they totally agree with the statement "La gracia de tomar alcohol es emborracharse" (The point about drinking alcohol is to get drunk). In what follows, the reader should bear in mind that this article is of a tongue-in-cheek humorous nature without taking ourselves too seriously.
What kind of fool would believe in that statement? If we talking about fools, could it be lower-class uneducated louts? In the next chart, we show the agree rate by socio-economic level and educational achievement. For socio-economic level (SES 6 is upper class whereas SES 2 is lower class), the relationship is monotone. For educational achievement, the relationship is not completely monotonic. For example, the group of "university incompletes" breaks the trend. Why? Is this because these are current university students? Or are these people who never graduated because of their interest in something else other than studies? We don't know.
(source: 2003 TGI-EGM Colombia)
In the chart below, we show the agree rates by age/sex groups. The bad news is that the highest agree rate occurs among juvenile males (see also The "Vices" Among Latin American Youth) while their mothers and grandmothers are appalled. Is this true? We think so.
A marketer may be less concerned about the ethics of selling alcohol for people to get stone-blind drunk than the practical knowledge of just what people prefer to drink in order to become drunk. Before showing any data, what would be your guess? Here is an article on an age-old Colombian drink (AP via Miami Herald):
Ever since the mid-1600s, when the king of Spain tried to ban it, aguardiente has been Colombia's beloved booze. Drunk from crystal shot glasses in wood-paneled lounges or from plastic cups in honky-tonks, aguardiente knows no class boundaries. ``What am I without aguardiente? I'm a nation without people, a tree without roots,'' a Colombian living in the United States once lamented in a now-famous poem.
Andean farm workers often carry a flask to ward off the frosty air. Step into a bar, and among the beer guzzlers and whiskey sippers you'll see people knocking back shots of the sweet anise-flavored liquor. ''It's not a sipping drink. You get a table and a bottle and sit there until it's done,'' said Pablo Robledo of the Caldas Liquor Industry, which produces Cristal aguardiente, a best-selling brand.
Time was, you couldn't get Colombians off aguardiente. Colombia's Spanish colonial rulers banned aguardiente in 1693, fearing it led to moral decay. The colonists ignored the ban. In 1700, the Spanish crown admitted defeat, and monopolized the industry. The colonists didn't much like his majesty muscling in, and scattered rebellions erupted across the land, but the controls remained tight until Colombia won independence in 1810. Many Colombians can sing by heart a song that is almost as sappy as the drink itself: ``Give me an aguardiente, made of the sugar cane of my valleys and the anise of my mountains. Don't serve me a drink from abroad which is expensive and doesn't taste as good.''
But today, aguardiente is facing competition from beer, which costs about the same; rum, which is only slightly costlier; and imported wines and spirits, which are less expensive with the easing of trade tariffs.
The following chart shows the consumption incidences of various alcoholic beverages. While beer may be most popular, it is admittedly not easy to become drunk on beer. In second place, we find the Colombian staple, aguardiente.
But our question is not about consumption incidences. We were looking at just who thinks that the point of consuming alcohol is to get drunk. In the next chart, we show the agree rate with our opinion statement by consumption behavior. The agree rate increases with consumption volume. We suppose that this should be expected, since heavy consumption presumably correlates with drunkenness and, we should add, hangovers. Of the beverage types, somehow tequila rose to the top, followed by vodka.
We ran a small survey among our Colombian acquaintances. Before anything, we asked, "If you have to get drunk in a hurry, what would you drink?" The universal answer was, "Aguardiente." What about tequila? Answer: Too complicated with the salt and lime. Then we showed them this chart and asked for an explanation. Without fail, they said that Colombians must have built up tolerance to aguardiente through repeated use. Is that true? We don't know ...
(posted by Roland Soong, 3/24/2004)


And in the moment they paused they breathed in deep and opened their eyes to a world forgotten, a slower more enjoyable place.
We drove, we drank, we ate, we laughed.
We stopped, we relaxed, we appreciated.
What a beautiful haven you have created.
Time is like the waves of the ocean that surrounds you, once passed it will never pass again and memories are etched into our minds – make a mark on the world, on people, friends and family. It is the only chance to make a difference. And this has been a lovely trip that has been forever etched into our lives. Rebecca and Jack, Thank You!
What an absolutely stunning and chic room. I had a very enjoyable stay in Launceston here with Hatherley Birrell.
The room is gorgeous and the host kind and hospitable – thank you.
I have enjoyed the wine and breakfast. Highly recommend this for a subsequent stay. Had so much fun in Tasmania!
Wow what a beautiful room. We loved it so much! Thank you for making our wedding night so special.
Thank you for 3 wonderful days and nights to reconnect with each other.
37 years later and I still 'like him' – a lot.
Your home is magnificent, Thank you for sharing.
What an amazing start to our Tasmania trip! Perfect! The rest of the place has a lot to live up to!
Such a wonderful, sumptuous room we listened to Bob Dylan and drank in the atmosphere. The underfloor heating and spa bath are all the simple things that keep a wife happy on her travels.
We will never forget where we spent our one year wedding anniversary.
Thank you for a gorgeous stay down here in Launceston – an absolutely stunning room! Much love.
A wonderful day at Agfest … cows, tractors and horses…then swapping our blunnies and jeans for elegant evening wear to relax and recover in the sumptuous Ballroom – what a treat to enjoy such beautiful surroundings! Thank you so much!


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Poincaré, Jules Henri | Article about Poincaré, Jules Henri by The Free Dictionary
https://encyclopedia2.thefreedictionary.com/Poincar%c3%a9%2c+Jules+Henri
(zhül äNrē` pwăNkärā`), 1854–1912, French mathematician, physicist, and author. He was from 1881 connected with the faculty of sciences at the Univ. of Paris. One of the greatest mathematicians of his age, Poincaré, by research in the theory of functions, especially the automorphic, Fuchsian, and Abelian functions, enlarged the field of mathematical physics. He did notable work also in differential equations and celestial mechanics, particularly the problem of three or more bodies moving under their mutual gravitational attractions. Poincaré not only made important contributions across the full range of mathematics, both pure and applied, but also wrote extensively on the philosophy of science. He was elected to the Academy of Sciences in 1887, became its president in 1906, and was elected to the Academie Française in 1909. His works include Les Méthodes nouvelles de la mécanique céleste (3 vol., 1892–99; tr., 3 vol., 1967) and three works (1902, 1904, 1908) published in English as The Foundations of Science (1913, repr. 1946).
Born Apr. 29, 1854, in Nancy; died July 17, 1912, in Paris. French mathematician. Member of the Académie des Sciences (1887).
Poincaré studied in Paris at the Ecole Polytechnique from 1873 to 1875 and at the Ecole Nationale Supérieure des Mines from 1875 to 1879. Beginning in 1886 he was a professor at the University of Paris. He became a member of the Bureau des Longitudes in 1893. Poincaré's work in mathematics marked the end of the classical period and cleared the way for the development of the new mathematics, wherein not only quantitative relations but facts having a qualitative character are established.
An important group of studies by Poincaré dealt with the theory of differential equations. Poincaré studied the expansion of solutions of differential equations in terms of the initial conditions and small parameters, and he proved that certain series expressing the solutions of partial differential equations are asymptotic. His doctoral dissertation investigated the singular points of a system of differential equations. Poincaré then wrote a series of papers under the general title "On Curves Determined by Differential Equations" (1880). In these studies, he constructed the qualitative theory of differential equations, investigated the shape of integral curves in the plane, provided a classification of singular points, and investigated limit cycles, the distribution of integral curves on the surface of a torus, and certain properties of integral curves in n-dimensional space. He applied his investigations to the three-body problem and studied the periodic solutions of the problem and the asymptotic behavior of the solutions. He introduced methods using small parameters, fixed points, and variational equations and developed a theory of integral invariants.
Poincaré also wrote a number of important papers in celestial mechanics on the stability of motion and on the figures of equilibrium of a rotating fluid mass held together by the gravitation of its particles. His work in celestial mechanics was often characterized by a lack of rigor; for example, he made use of arguments by analogy. A. M. Liapunov was the first to make a rigorous investigation of the problems mentioned.
Poincaré was led by his investigation of ordinary differential equations with algebraic coefficients to the study of new classes of transcendental functions called automorphic functions. He proved the existence of automorphic functions with a given fundamental domain, constructed series for the functions, proved an addition theorem, and showed that algebraic curves could be uniformized. He used Lobachevskian geometry in developing his theory of automorphic functions. For functions of several complex variables his results include the construction of a theory of integrals analogous to the Cauchy integral and the demonstration that an everywhere meromorphic function of two complex variables can be represented as the quotient of two entire functions. These investigations and his work on the qualitative theory of differential equations drew Poincaré's attention to topology. Poincaré introduced such fundamental concepts of combinatorial topology as Betti numbers and the fundamental group. He proved the Euler-Poincaré formula, which gives the relation between the number of edges, vertices, and faces (of any dimension) of an n-dimensional polytope. Finally, he gave the first intuitive formulation of the general concept of dimension.
In mathematical physics, Poincaré investigated the vibrations of three-dimensional continua. He also studied a number of problems in such areas as thermal conductivity, potential theory, and electromagnetic oscillations. He is the author of papers on the foundations of the Dirichlet principle, for which he developed the "sweeping out," or balayage, process. Poincaré made a profound comparative analysis of the then current theories of optical and electromagnetic phenomena. In 1905 he wrote the paper "On the Dynamics of the Electron," which was published the following year. In this paper he developed the mathematical consequences of the "relativity postulate" independently of A. Einstein.
Poincaré's scientific work in the last decade of his life took place at a time when a revolution had begun in natural science. This fact undoubtedly determined his interest in that period in the philosophy of science and in the methodology of scientific cognition. A brief summary of his philosophical views follows.
The fundamental statements, that is, the principles and laws, of any scientific theory are neither synthetic a priori truths, as I. Kant had maintained, nor models or reflections of objective reality, as they had been for the 18th-century materialists. Rather, they are conventions, and the sole absolute criterion for these conventions is consistency. Which statement we choose from a set of possible statements is, in general, arbitrary if we ignore the circumstances under which the statement is used. In actual fact, however, we are guided by this latter consideration. The selection of fundamental principles or laws is thus limited, on the one hand, by the need of our minds for maximally simple theories and, on the other hand, by the necessity of the theories' successful use. These requirements permit a certain freedom of choice because of their relative nature. This philosophical doctrine of Poincaré subsequently became known as conventionalism. A critique of Poincaré's philosophical views was given by V. I. Lenin in Materialism and Empiriocriticism.
Oeuvres, vols. 1–11. Paris, 1916–56.
Les Méthodes nouvelles de la mécanique céleste, vols. 1–3. Paris, 1892–97.
Leçons de mécanique céleste, vols. 1–3. Paris, 1905–10.
In Russian translation:
Tsennost' nauki. Moscow, 1906.
Nauka i gipoteza. St. Petersburg, 1906.
Nauka i metod. St Petersburg, 1910.
Poslednie mysli. Petrograd, 1923.
O krivykh, opredeliaemykh differentsial'nymi uravneniiami. Moscow-Leningrad, 1947.
lzbr. trudy, vols. 1–3. Moscow, 1971–74.
Acta mathematica, 1921–23, vols. 38–39. (Devoted to Poincaré's life and work.)
Poincaré, Jules Henri
poi dance
Poiarkov, Vasilii
Poiarkov, Vasilii Danilovich
Poiarkovo
Poiasovyi Kamen
poidometer
Poienesti
poikile
poikilitic
poikiloblast
poikiloblastic
poikilocrystallic
poikilocytosis
Poincare conjecture
Poincaré equation
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Poincaré expansion
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Poincaré group
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Poincare polynomial
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Poincaré recurrence
Poincare recurrence theorem
Poincarè recurrence theorem
Poincare recurrence time
Poincaré recurrence time
Poincare Sphere
Poincare theorem
Poincaré theorem
Poincare's Conjecture
Poincaré's equation
Poincare's recurrence theorem
Poincaré's recurrence theorem
Poincare's theorem
Poincaré's theorem
Poincare, Jules Henri
Poincare, Raymond
Poincaritis
Poinciana Civic Organization
Poinciana gilliesii
Poinciana pulcherrima
Poinciana regia
Poind
poinded
Poinder
Poindexter
poinding
poinding of the ground


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Listen: Brian Jones, Sam Burnett, Jim Morrison discussed on WGN Programming
"This very, very intriguing. Talk with the co owner of the Chicago Dogs. Baseball team will talk about grilling and spices with it being the Fourth of July weekend at Awesome, Really good information. I'm hoping we're going to get I've got a very, very cool story to share with you. It's a really a great American success story. And I think when you hear this story you're gonna call. Oh, wow. That is so cool. We're going to hear from the founder of a very cool brewery as well. They've got a great theme, and we're going to talk about holiday movies so kind of something for everyone. Really appreciate you being here. Some things that happened on this date in history in 1969. Brian Jones of the Rolling Stones was found dead at the age of 27. He was discovered motionless. At the bottom of his swimming pool at Catch Furred Farm in England. It was pronounced dead on arrival at the hospital at the age of 27 a drowning, according to the coroner's report. They later changed that. To death by misadventure, noting his liver and heart were enlarged by drug and alcohol abuse. It was on this date in 1971 as well that Jim Morrison was found dead in the bathtub of his Paris apartment, apparently of heart failure, becoming another member of the notorious 27. Club. Those who died at the age of 27. French officials found no official evidence of foul play, and no autopsy was performed. In 2000 and seven. The story gets more interesting because Paris Club owner Sam Burnett published a book claiming that Morrison died of a heroin overdose at his nightclub and was carried back to his apartment placed in the bathtub to cover up the real reason for his death. So we wanted to get those things out of the way there. Not negative, but kind of big names that died on this day. Members of the 27 club, I'm gonna lighten things up. It is also American redneck Day. This is true. I'm not making this up. The term basically applied to those living in the South. Characterized as an educated truck driving uber patriotic gun owning backward. Some were labeled as other things as well that we are not going to get into, but it is actually a physical. The pilot, it's a definite thing. American redneck date. You have to mention Jack Jeff Foxworthy. When we talk about that, who made a good living off of the phrase? You might be a redneck if Can't forget about him. All right, so we're going to talk to a couple podcasters next as we get things going here at 7 20 w g. N."
WGN Radio
Brian Jones, Sam Burnett, Jim Morrison discussed on WGN Programming
WGN Programming
1 year ago | WGN Radio
Brian Jones Sam Burnett Jim Morrison Jack Jeff Foxworthy 1971 1969 Chicago Dogs 2000 Paris Club Morrison 7 20 W G. N. Catch Furred Farm Paris England 27 Rolling Stones 27. Club Fourth Of July French Redneck Day
This very, very intriguing. Talk with the co owner of the Chicago Dogs. Baseball team will talk about grilling and spices with it being the Fourth of July weekend at Awesome, Really good information. I'm hoping we're going to get I've got a very, very cool story to share with you. It's a really a great American success story. And I think when you hear this story you're gonna call. Oh, wow. That is so cool. We're going to hear from the founder of a very cool brewery as well. They've got a great theme, and we're going to talk about holiday movies so kind of something for everyone. Really appreciate you being here. Some things that happened on this date in history in 1969. Brian Jones of the Rolling Stones was found dead at the age of 27. He was discovered motionless. At the bottom of his swimming pool at Catch Furred Farm in England. It was pronounced dead on arrival at the hospital at the age of 27 a drowning, according to the coroner's report. They later changed that. To death by misadventure, noting his liver and heart were enlarged by drug and alcohol abuse. It was on this date in 1971 as well that Jim Morrison was found dead in the bathtub of his Paris apartment, apparently of heart failure, becoming another member of the notorious 27. Club. Those who died at the age of 27. French officials found no official evidence of foul play, and no autopsy was performed. In 2000 and seven. The story gets more interesting because Paris Club owner Sam Burnett published a book claiming that Morrison died of a heroin overdose at his nightclub and was carried back to his apartment placed in the bathtub to cover up the real reason for his death. So we wanted to get those things out of the way there. Not negative, but kind of big names that died on this day. Members of the 27 club, I'm gonna lighten things up. It is also American redneck Day. This is true. I'm not making this up. The term basically applied to those living in the South. Characterized as an educated truck driving uber patriotic gun owning backward. Some were labeled as other things as well that we are not going to get into, but it is actually a physical. The pilot, it's a definite thing. American redneck date. You have to mention Jack Jeff Foxworthy. When we talk about that, who made a good living off of the phrase? You might be a redneck if Can't forget about him. All right, so we're going to talk to a couple podcasters next as we get things going here at 7 20 w g. N.


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First Lines: There were two reasons why William South did not want to be on the murder team. The first was that it was October. The migrating birds had begun arriving on the coast. The second was that, though nobody knew, he was a murderer himself.
William South is a policeman and an avid birdwatcher. He is trusted and respected by all. When he's not on the job, he keeps himself to himself, watching the birds he loves so much-- sometimes with his neighbor. When that neighbor is found brutally murdered, the lead officer on the investigation is Detective Sergeant Alexandra Cupidi, a recent transfer from London. She insists on having South on the team because of his knowledge of the area and of the victim, although South learns that he really didn't know much about the dead man after all.
As the investigation progresses, all signs point to the killer being someone from South's childhood in Northern Ireland, a man who is the only person who can tie William to the past he's worked so hard to forget. The more South is drawn into the investigation, the harder he has to work to keep his own connections to the suspect, and his past, a secret.
The first four lines of The Birdwatcher are stunning. You know immediately that William South is a killer, but as you read and make your way around South's mind, you can't believe that he is. And then you learn more. And more. South is a completely sympathetic character in a vivid, atmospheric setting, tasked with finding a killer, and teamed with the questionable DS Alexandra Cupidi. I first learned about this book after reading the synopsis of Salt Lane and discovering that it was the second book in the Alexandra Cupidi series. I had a feeling that I definitely wanted to start at the beginning, so I got a copy of The Birdwatcher. I'm glad I did because I was only a few pages into the story when I knew that I was reading something very special.
It wasn't just about a mystery that keeps you guessing. It wasn't just about the remoteness and loneliness of a landscape that mirrored the mind of the main character. It was about a troubled teenage girl who proved to be the one person lonely William South could open up to. And it was about a totally infuriating lead investigator. As I read The Birdwatcher, I wondered if I really wanted to go on to read Salt Lane. You see, I couldn't stand Alexandra Cupidi. She's the type of "force of nature" that I want to head in the opposite direction from. Cupidi presumes much when it comes to William South. She commandeers his house and turns it into their base of operations, and she also turns him into a babysitter. It's almost as if she went out of her way not to endear herself to me. And it worked. But... she's a fine investigator.
I think William Shaw is a puppetmaster when it comes to storytelling. Keep your eye on him. I was completely drawn into his tale, and although the ending was inevitable, I loved the book, and nothing is going to keep me away from the second Alexandra Cupidi mystery-- not even Cupidi herself.
Those first lines are so intriguing, Cathy! And I do like novels that give the reader a strong sense of place and atmosphere. Most definitely it sounds as though this is one them. One for me to look into, I think.
I read about this book a while back when another blogger loved it. Can't think who it was? Maybe Cath at read warbler. Anyway, I got on audio, but haven't listened to it yet. I can see that I need to move it up the list. I'm so glad that you explained that you detested the investigator, but that you'll be racing to read the second book. Now I've got to read them both!
She's the type of train wreck character that you just HAVE to know more about, but if she isn't made a bit more sympathetic in Salt Lane, I'm doubting that I'll want to continue with the series.
Yes, it was, as Kay said, me who read it several months ago and really enjoyed it. My big problem is exactly what you said, I'm not sure I want to read Salt Lane as I didn't like Cupidi at all. So I'm not sure... maybe wait and see what you think. LOL!
I guess I must read this book after seeing this rave review.
Who can resist a review like this? Now, I'll have to see about Cupidi.
I'd be interested to see what you think of her, Kathy!
Intriguing which I gets better as you read more. Thanks for the review.


text:
The Inaugural London Gala in 2013 raised over £1.2 million for the Novak Djokovic Foundation to support vulnerable and disadvantaged children in Djokovic's native Serbia. The evening drew celebrities, models, and royalty alike and featured a live auction of one of a kind experiences and collectables such as a yacht getaway with Goldie Hawn and Kate Hudson, a guitar signed by Ronnie Wood, and a holiday at Richard Branson's private island.
Famed mentalist Lior Suchard stunned the crowd with a performance and the evening also featured a mini tennis match with Goldie Hawn and Kate Hudson participating. Attendees included: Goldie Hawn, Kate Hudson, Naomi Campbell, Ronnie Wood, Gerard Butler, Jonathan Ross, Matt Bellamy, Boris Becker, Sir Richard Branson, Sarah Ferguson, Duchess of York, Princess Beatrice, and Princess Eugenie.
AAB Productions
Novak Djokovic Foundation New York Gala
For two years beginning in 2012, the Novak Djokovic Foundation held its New York Gala raising over $3.9 million for preschool programs in Serbia. Celebrities and leading names in the worlds of sport, fashion and music came out to support the event held following the US Open and in the midst of New York Fashion week. The event featured a dinner, auction, and performances. Ricky Gervais, Goldie Hawn, Naomi Campbell, and Karolina Kurkova joined on stage to help auction off some one-of-a-kind experiences including a private tennis match with Novak Djokovic and an opportunity to attend a fashion show with Anna Wintour.
Past performers include Theophilus London, pianist ELEW and mentalist Lior Suchard. Attendees included: Adriana Lima, Anna Wintour, A$AP Rocky, Goldie Hawn, John McEnroe, Karlie Kloss, Meghan Markle, Naomi Campbell, Nicky Hilton, Ricky Gervais, and Toni Garrn
64 Allen Street | 5th Floor | New York NY 10002 | Tel +1 212.219.0297 | Fax +1 646.607.2767 | events@aabproductions.com | Twitter | Instagram


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The 'Lucky' pulled up to a city bus stop at the edge of Dorchester Square. Cameron walked up the curb past the front of the bus. He fixated on the green dome of the building across the square, the girth of which towered over the park.
"King of the world," said Cameron.
"Excuse me," said Nicole.
"Cathedrale Marie-Reine-du-Monde," said Cameron. He pointed at the columned structure, the statues lining the parapet. "I always thought of this church as a mini Saint Peter's. It's basically Saint Peter's on a smaller scale."
"What do you think of it now?"
"Its name. It is the Mary, Queen of the world Cathedral. The Rex Mundi cathedral."
"Ah, I see," said Marie gazing at the basilica. She braced her elbow in her hand and tapped her chin with the fingertips of the other. "The name means nothing."
"All cathedrals are creations of Rex Mundi," said Nicole.
"You don't say," said Cameron.
"As are all things in the material world."
"Ok," said Cameron. He shifted his body away from the park to Marie. "So, do you know where we are to meet the woman?"
"The person we must meet will not be available until this evening," said Marie.
Still early, Cameron suggested they eat before the meeting. They went around the corner to a large hotel and entered the restaurant. After eating only fruit all day, he had worked up an appetite. He ordered the salmon with a glass of wine. Marie and Nicole asked for the same.
"You really do eat fish?" asked Cameron when the waiter stepped away.
"I told you it is part of the old way," said Nicole.
"We do not eat meat or byproducts of reproduction like eggs, milk, cheese. The old beliefs are that fish spontaneously appear in the water. So fish is allowed," said Marie.


Sketch book: Spiral-bound Mead Academie sketch book with 8 1/2″ x 11″ pages. The pages are perforated so you can tear them out neatly. This is useful for me because I do almost all of my outlining, note-taking and planning using Mind Mapping (aka idea mapping), a visual form of writing. Unlined paper is essential for this way of working. The 8 1/2 x 11 size is important so sheets will fit in standard file folders and cabinets — most sketch book paper sizes are too big.
Pocket notebook: Custom-made spiral notebook made with unlined paper and sized to fit in a shirt pocket. Especially critical for jotting down ideas anywhere I go — as you know, ideas can come to you at any time and you need a medium to capture them right away. Again, the unlined paper is important, as I often make these notes in visual format. I have these custom-made at an office supply store such as Office Max or Staples.
Shirt pocket pouch: This was custom-made by a designer who works with my wife at Trader Joe's. Kim originally made it as kind of a joke because I told Virginia I needed a pocket protector to hold all of my writing instruments (I am mercilessly ridiculed by everyone I know for carrying all this stuff in my shirt pocket). The first thing I did when I received the pouch was cut off the front flap, the part that is supposed to protect your pocket. That doesn't matter much to me. What does matter is having all of my writing instruments in one container that I can quickly and easily take in and out of my shirt pocket. The pouch is made of suede, so it doesn't fall out of my pocket easily.
Pens: I carry three pens in my shirt pocket, plus a small highlighter and a stylus that I can use on my smartphone or tablet for special text-entry tasks. The pens are all very specialized and could be considered individual tools in themselves. The most important is a Coleto five-color gel pen I bought from JetPens. It's a great piece of technology for someone who likes to take multi-color visual notes. It's not disposable like the cheap multi-color pens you can buy in office supply stores. When a color runs out, you install a refill, and the refill process is not too difficult. Another pen I carry is a useful Zebra combination mechanical pencil and ballpoint pen with both red and black cartridges. It also has an eraser, which you don't always get with multipens that have pencil cartridges. The third pen is an 005 extra-fine marker pen. I alternate between the Pigma Micron and the Prismacolor Premier, both of which I like. I use these markers principally for making marginal notes in books and journals — plus any time I need to write something in a very small space. These pens are very legible and don't bleed.
Cargo pants: Just gotta say it. If God hadn't wanted us to carry a lot of stuff, he wouldn't have given us cargo pants.
Digital audio content: I read a lot, but digital audio (and books on tape before that) has made it possible for me to consume a lot more content, both fiction and non-fiction. Right now, I use an iPod Nano just because it is a reasonably robust and rugged technology. My most important content comes via a monthly subscription to Audible.com, which allows me two audio books a month for a set fee. Over the past year or two, podcasts have become more important to me as content sources. Because I use the iPod, I synch with iTunes, but Audible has its own Audible Manager application, which has improved over the years and synchs with many brands of digital audio players. I listen to audio content when I am driving any significant distance, and this format for content is a tremendous incentive for me to exercise every day.
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DAVIDsTEA opens for business in Fashion Outlets of Chicago!
Located just across I294 from O'Hare, this vibrant new mall offers a great mix of retailers to please any shopper. Macon just completed the newest addition to the mix – DAVIDsTEA – where you can choose from over 150 types of tea, including exclusive blends, limited edition seasonal collections, traditional straight teas and exotic infusions from around the globe. Not to mention the largest collection of organic teas and infusions in North America. Check out the new store design and be on the lookout for the new store opening soon in Oakbrook Mall!
2 years, 4 months ago Comments Off on DAVIDsTEA opens for business in Fashion Outlets of Chicago!
Click HERE to see the full DNA Info story and check out the slideshow below of photos from throughout the project.
Wendy's at 4100 S Pulaski is now open for business!
The new ground-up drive thru is located just south of I-55 on Pulaski. It is the first LEED Certified project for Wendy's in the Chicagoland area.


Introducing Churro Poppers with Dipping Sauce…drool.
He randomly tags me in Facebook videos of homemade churro recipes…droppin the hint left and right. And I finally caught on. So these Churro Poppers are for you babe.
Now I recognize that we promote "healthy living" on this blog and usually post healthy recipes. But to us, healthy living means finding balance…enjoying Churro Poppers with Dipping Sauce from time to time without feeling even an inkling of guilt. So no, these are not "healthified." Well, they are baked instead of fried, so I guess they are "healthier" in a way, but that's because we wanted this to be a relatively simple recipe with an easy clean up.
But hey, if you want to fry them, all power to ya.
The second is a maple-vanilla dipping sauce. We used pure maple extract in this one to give it that strong maple flavaaah. (Most grocery stores carry it by the vanilla extract or you can order it here).
So get in touch with the inner child in you…the one that begged for churros at the circus, county fair and basketball game. You're the adult now. You get to make that decision to eat Churro Poppers with Dipping Sauce and feel dang good about it.
In a small saucepan add half and half and butter. Heat over low heat until butter is melted.
Add chocolate chips and continue to heat until melted, stirring continuously.
Remove from heat and add rest of ingredients. Stir until incorporated, cool and serve.
Add all ingredients in a small bowl and mix until incorporated.
Mix together flour, baking powder, salt, cinnamon and nutmeg in a medium bowl. Set aside.
In the bowl of an electric mixture, beat together sugar and butter until fluffy, about 2-3 minutes.
Add half the dry ingredients, mix and then add the half and half. Add rest of the dry ingredients and mix just until incorporated.
Use a Tbsp. to scoop dough into muffin tin holes.
Bake 15-18 minutes, until just golden brown.
While churros are baking, melt butter in a bowl. Combine sugar and cinnamon in another bowl.
When churros come out of the oven, immediately remove from the pan and dip each one in butter first and then roll in cinnamon-sugar coating until completely coated.
Dip into sauce and enjoy!
Haha we had a similar problem when we made them 😉 Definitely a splurge treat!
I made these and are wonderful!! I dipped mine in carmel made in my slow cooker, so easy.
These are SO YUMMMY! I only had heavy cream so I used that instead of half and half (no ones complaining about some extra fat) and they were amazing. Everyone loved them!!


I feel inclined at the start of this review to depart briefly from my usual structure, as I think this film presents an unusual and fascinating case. There is significant value in taking a moment simply to appreciate the unique story of the filmmaker who crafted Columbus. Kogonada didn't pave the path to his first feature film in the traditional way. He didn't work his way up through the stages of production until he was finally given a directors chair. He made a name for himself through a passion for film and through his popular series of online video essays exploring the patterns and styles of influential filmmakers from the past. It is noteworthy that his deep appreciation of film as art, and particularly as a visual medium, leads to this poetic and thought provoking debut.
Columbus tells the story of Jin (John Cho) and Casey (Haley Lu Richardson) as two young people who encounter each other while the former is staying in Columbus to look after his sick father. Though the pair know each other for only a short time, they form a quick and intimate bond. The dynamic between the two main characters in the film is very unconventional and doesn't take on the passionate romance narrative that the viewer would necessarily expect given the plot. Still, the connection between the two is more loudly amplified through incredible emotional performances that reveal not just written characters, but real humans experiencing real pain and suffering.
Visually, Columbus expresses itself largely through its physical environment, and more specifically through architecture. Jin's father is a renowned architect and Casey has a particular interest in architecture. It is not an accident that the town of Columbus is considered an architectural "Mecca", as the film states, and much of Columbus' imagery is derived directly from the beautiful and unique buildings that occupy the city. Kogonada explores themes of symmetry and asymmetry throughout the film with verbal, visual, and thematic queues spurred by the architecture. Similarly, he delves deep into the topic of modernism, a theme which floats close to the surface throughout the film's run time.
In reflecting on the film, it strikes me just how simple the whole thing is. I could sum up the plot in only a few sentences, which may lead to some audiences perceiving Columbus as "slow", but it was so intimate and engaging throughout that the viewer becomes more drawn into the details of the individual moments than the broader scope of the plot. Even seemingly uneventful moments have an incredible depth of emotion clearly attached, and Kogonada certainly knows how to point a camera to make every single frame of the film undeniably more interesting than if he had stuck to a more traditional visual style.
I have little doubt after seeing Columbus that we are witnessing the beginnings of a brilliant career. But more than that, it seems that we might be witnessing the first work of an entirely unique artist. In viewing the film, it is exceedingly obvious that any ordinary filmmaker could've constructed this story in a way that would've been perfectly acceptable and palatable to audiences. But I'm not sure that many could've taken these precise ideas and built them into the expressive and artistic work that appears on the screen. I'm not sure what direction Kogonada will take next or whether wider audiences will respond to Columbus in the way that art film enthusiasts have, but needless to say I am very excited to find out.


I am a wife and a stay at home mom and a follower of Christ. I live in the South and I love my home and my family and I think my church is an incredible place to be. I am very blessed. Every single day I am amazed at God's great love and redeeming power. My greatest thrill is encouraging others with stories of how He has proved Himself faithful over and over in my life...which makes it a very sweet life!
"My willingness to believe God and to walk in faith now in the things that don't seem like such a big deal—that willingness to walk by faith is an indicator of where my heart will be later in life. It's a determining factor in my long-term usefulness to God and His kingdom. "
~Nancy Leigh DeMoss, from her Revive Our Hearts radio broadcast of 3/16/09 titled "The Trap of Unbelief"


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Home › News › Cat On Leash Gets A Little Lost And Ends Up On Edge Of Bridge
Cat On Leash Gets A Little Lost And Ends Up On Edge Of Bridge
People in a building overlooking the Bay Bridge in San Francisco were looking out the window when they spotted something strange on a ledge of the bridge. After a few moments, they suddenly realized that it was a cat wearing a harness and leash, and he was definitely very stuck.
The onlookers knew that the cat was in desperate need of help and immediately contacted San Francisco Animal Care & Control (SF ACC), who then sprang into action.
"Our animal control officers (Sgt. Kent and Ofc. Sherwood) contacted the California Highway Patrol and Caltrans (they help stranded motorists on the bridge) to help them," Deb Campbell, of SF ACC, told The Dodo. "Those agencies stopped traffic so our ACOs could work safely."
As the officers peered down at the very stuck cat, they were surprised to see that he didn't seem scared or concerned, and instead was just kind of hanging out. Still, they knew they needed to get him to safety as soon as possible, as it was a 300-foot drop from where he was down to the road below.
While one officer took hold of the leash, the other officer used a net to very carefully secure the cat and then pull him up off the ledge and to safety at last.
Throughout the entire rescue, the cat remained unfazed, as if he had meant to be on that very dangerous ledge all along.
"He was calm during the rescue and doesn't seem rattled by the experience," Campbell said.
The cat, who was determined to be around 6 years old, was in pretty good condition, besides having some fleas and a few scratches. He's recovering safely in the care of SF ACC, and his rescuers are now embarking on a search to try and find his family.
"Nobody has claimed him yet," Campbell said. "We've had inquiries from people who think he may be their cat, but no matches yet."
It's still a mystery as to why the adventurous cat was on the bridge in the first place or where his family may be, but for now, he's loving his stay at the shelter with all his new friends. He's a super friendly, confident guy who loves all the attention he's getting. His rescuers are hoping that by posting pictures of him on social media, his family may eventually recognize him, and they can get him back home where he belongs.
"He's very friendly and it was hard to get photos as he just wanted to cuddle," Campbell said.
If you think you know where this cat belongs, you can contact SF ACC.


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\section*{Version fran\c{c}aise abr\'eg\'ee}

\selectlanguage{english}

\section{Introduction}
\label{sec:intro}

Earth's atmosphere is opaque to many types of electromagnetic radiation, including $\gamma$ rays.  Direct detection of these energetic photons therefore requires instruments in space.  Although $\gamma$ rays represent a broad swath of the electromagnetic spectrum, essentially everything above about 0.1 MeV, this article concentrates on the band from $\sim$100 MeV to $\sim$100 GeV, where satellite detectors have been particularly successful in revealing high-energy, nonthermal phenomena in the Universe.

The material is organized in three parts: (1) the physics of pair production and multiple Coulomb scattering, which are central to these detectors; (2) the challenges of designing a $\gamma$-ray detector within the constraints of launching and operating an instrument in space; and (3) the  implementation of the design principles using technologies of two eras, represented by the Energetic Gamma Ray Experiment Telescope (EGRET) on the Compton Gamma Ray Observatory (CGRO) and the Large Area Telescope (LAT) on the Fermi Gamma-ray Space Telescope (Fermi).

\section{Basic Principles}

The goal of any astrophysical instrument is to measure the properties of the incoming radiation: arrival direction, arrival time, energy, and possibly polarization.   Photons with energy E $>$ 100 MeV interact almost exclusively through the process of electron-positron pair production: $\gamma$ $\rightarrow$  $e^+$ +  $e^-$.  The photon itself ceases to  exist; therefore reflection (mirrors) and refraction (lenses) are not applicable to $\gamma$-ray detectors.  The properties of the incident $\gamma$ ray can only be derived from measurements of the two charged particles. This basic principle explains why all high-energy $\gamma$-ray detectors use instrumentation developed for nuclear and particle physics.

Pair production cannot occur in free space; that would violate conservation of energy and momentum.  The most common agent to enable pair production is an atomic nucleus, which absorbs some of the momentum, but almost none of the energy.  The combined energy of the electron and positron is therefore a good approximation to the total energy of the original $\gamma$ ray.

\begin{figure}[!t]
 \centering
 \includegraphics[width=7.5cm]{SPACE_Fig1.eps}
 \caption{Probability per radiation length of lead for photons with energy W in eV to interact: $\sigma_{\mathrm{c}}$ is the probability for Compton scattering; $\sigma_{\mathrm{p}}$ is the probability for pair production. Reprinted figure with
permission from \cite{Rossi_Greisen}, copyright 1941
by the American Physical Society.}
 \label{fig:Pair_production}
\end{figure}

The first requirement for a $\gamma$-ray detector is some material to act as a converter.
Figure~\ref{fig:Pair_production} shows the probability for photon interactions in lead as a function of energy.  For one radiation length of material, a large fraction of the high-energy photons can be converted to pairs.  Because higher-Z materials have shorter radiation lengths (in g cm$^{-2}$), choosing such materials minimizes the mass of material needed to achieve a reasonable probability of having the $\gamma$ rays detected. See \cite{Rossi},\cite{Olive} for a detailed discussion of pair production and related electromagnetic processes.

Converting the $\gamma$ rays into electron-positron pairs is the easy part of building a detector.  Extracting the properties of the incident photons from the particle pair is harder.  Even so, two pieces of information are fairly straightforward to determine:  (1)  the arrival time of the photon can be measured by any detector, such as a scintillator, that is hit by either particle; and (2) the energy of the photon can be approximated by measuring the energies of the two particles in some sort of energy calorimeter, correcting for energy losses in any material they pass through.

The bigger challenge is determining the arrival direction of the incident $\gamma$ ray, an essential bit of information for astrophysics.  Because the $e^+$ and  $e^-$ carry most of the energy of the photon (at least for energies well above the combined rest mass energies of the two particles), their paths after the point of conversion can be used to derive this direction.  The most probable opening angle, in radians, between the electron and positron can be approximated as \cite{Olsen}

\begin{equation}
\theta_{\mathrm{open}}=\frac{\mathrm{0.8}}{\mathrm{E_{\gamma}}}
\end{equation}

\noindent where $E_{\gamma}$ is the $\gamma$-ray energy in MeV. Above 100 MeV, this opening angle is relatively small (and decreases with increasing energy), allowing the track directions to be used to measure the photon arrival direction. The immediate requirement is therefore some sort of particle tracking detector.

The complication is the fact that these charged particles interact with the converter and any other material in their paths through multiple Coulomb scattering, which degrades the information about their initial directions.  In a Gaussian approximation, for electrons and positrons the root-mean-square scattering angle $\theta_0$ in radians projected on a plane (so the full space angle would be $\sqrt{\mathrm{2}}\theta_0$) is given by  \cite{Lynch}

\begin{equation}
\theta_0=\frac{\mathrm{13.6 MeV}}{\beta\mathrm{cp}}\sqrt{\mathrm{x/X_0}}\left[{\mathrm{1 + 0.038\ln{(x/X_0)}}}\right]
\end{equation}

\noindent where $\beta\mathrm{c}$ and p are the velocity and momentum of the particle, x is the thickness of the scattering material in g cm$^{-2}$, and X$_0$ is the radiation length.  The scattering in a thick converter quickly erases most of the information about the incident photon arrival direction. The high-Z, short-radiation-length material that is advantageous for enabling pair production is now a disadvantage because it aggravates the multiple Coulomb scattering.  The solution to this problem is to break the converter into multiple thin layers, interleaved with particle tracking detectors.  A generic instrument concept is shown in Figure~\ref{fig:generic}. Various implementations of this basic idea have been used in space $\gamma$-ray detectors.

\begin{figure}[!t]
 \centering
 \includegraphics[width=10.5cm]{SPACE_Fig2.eps}
 \caption{Generic space $\gamma$-ray detector}
 \label{fig:generic}
\end{figure}

Even harder to measure than the arrival direction of the $\gamma$ rays is their polarization, although polarization would be a valuable astrophysical diagnostic for objects such as pulsars, supernova remnants, active galactic nuclei and $\gamma$-ray bursts.  For linear polarization, information about the plane of polarization is carried through pair production into the plane of the electron-positron pair \cite{Maximon_Olsen}.  The effect, however, is small, and like the direction of the pair itself, the plane of the pair is easily distorted by multiple Coulomb scattering.  Nevertheless, polarization has been detected by pair production at accelerators, e.g. \cite{Barbiellini}. See \cite{Bloser}, \cite{Buehler}, \cite{Bernard}, and \cite{Hunter} for discussions of this topic in the context of possible space $\gamma$-ray instruments. At present, it is fair to say that polarization is an unrealized potential of space high-energy $\gamma$-ray detectors.

\section{Space Instrumentation Issues}

Applying the principles outlined in the previous section to a $\gamma$-ray detector in space involves a wide range of other considerations.  Many of these are logistical issues like mass, power, and money.  Others represent the challenges of the launch stresses and the space operating environment.  The most important design issue, however, is finding an efficient way to deal with the intense charged particle environment experienced by any space instrument.

\subsection{Background Radiation in Space}

Even within the protection offered by Earth's magnetic field, space is filled with intense radiation, including primary hadronic and leptonic cosmic rays, along with secondary protons, electrons,  neutrons, and $\gamma$ rays produced by cosmic-ray interactions in the atmosphere.  Figure~\ref{fig:Background} shows a typical background for a satellite in low-Earth orbit, based on modeling done for the Fermi Gamma-ray Space Telescope \cite{Pass7}.  The flux decrease for primary particles below 10 GeV reflects the geomagnetic cutoff.  Shown for comparison is the extragalactic $\gamma$-ray background, which is orders of magnitude less intense than the local background in this environment. Further, the background comes from all directions, since many of the secondary particles are coming up out of the atmosphere. Separating the cosmic $\gamma$ rays from all this unwanted radiation is the biggest problem in designing a successful space $\gamma$-ray instrument.

The primary approach to identifying the charged particle background is to surround the active detector with an anticoincidence detector, as illustrated in Figure~\ref{fig:generic}.  Plastic scintillator is the material of choice, because it has high efficiency for detection of charged particles but low probability of absorbing $\gamma$ rays.  A signal in this detector implies a charged particle that can be rejected, either in hardware or software triggering of the instrument.  Note that the anticoincidence detector cannot surround the entire instrument, because at GeV energies the $e^+$ and  $e^-$ produce showers, including penetrating particles that would produce self-veto.  Even with an extremely efficient anticoincidence detector, however, there will be some particles that will go undetected or enter through uncovered parts of the geometry and must be removed by other means.  Space $\gamma$-ray instruments use every bit of information about each potential pair production event to determine whether it was a real cosmic photon interaction. The ability of an instrument to produce analyzable data, separating signal from background, is a critical design element.

\begin{figure}[!t]
 \centering
 \includegraphics[width=15.5cm]{SPACE_Fig3.eps}
 \caption{Model of the Fermi orbital position and particle direction-averaged
    radiation intensities \cite{2004.CR_MODEL} sampled from a
    background simulation run. The intensity of the
    extragalactic $\gamma$-ray background (EGB - the heavy dashed line in the figure) measured by the Fermi LAT
    \cite{ExtraGalBkg} is shown for comparison. The event energy
    is reconstructed under the hypothesis of a downward-going $\gamma$ ray
    and in general does not represent the actual energy for hadrons.}
 \label{fig:Background}
\end{figure}

\subsection{Reaching and Surviving the Space Environment}

In addition to achieving science goals, the design of any space instrument must consider the realities of rocket launches and operating in space.  Rockets generate noise, vibrations, and large sustained acceleration.  Repairing an instrument once it is in space is essentially impossible.  Similarly, expendable supplies such as fuel, gas or cryogen are not likely to be replaced.  Durability is therefore a vital element of any space project.  Particularly in low-Earth orbit, a spacecraft faces a challenging thermal situation.  Many times each day, the satellite makes a transition from being in full Sun to facing exposure to the cold of deep space.  Thermal stresses, as well as changes in performance due to temperature variations, must be considered. All this must be done in a vacuum, where radiative transport, rather than conduction or convection, is the principal form of heat transfer.  The space radiation environment requires that electronic circuits be radiation-hardened to minimize failures.  Such design considerations are common to any space instrument.

As an example of the sort of trade-off required, consider natural micrometeoroids and human-generated space debris, a problem that has been exacerbated by some destructive collisions of satellites.  Micrometeoroid/space debris objects have a wide range of sizes, with potential impact velocities often reaching 20 km/s or more, compared to 1-2 km/s for a high-power rifle bullet. Such high velocities make even small projectiles dangerous to satellites\footnote{See http://esabase2.net/wp-content/uploads/2013/07/ESABASE2-Debris-Technical-Description.pdf}.  The outer element of a $\gamma$-ray detector, as noted above, is likely to be plastic scintillator, which must be shielded from light.  Putting a massive barrier outside the anticoincidence detector, however, negatively impacts the science, both by absorbing incoming photons and by acting as a $\gamma$-ray background source from inelastic collisions of cosmic-ray particles with the barrier material (producing neutral pions that decay immediately to $\gamma$ rays). The compromise is to use a low-Z multi-layer composite blanket that has a high probability of stopping projectiles of a size and velocity likely to hit the instrument during its lifetime.

\subsection{Practical Issues of Space Instrumentation}

No matter how excellent the scientific motivation, the ultimate existence of any satellite project depends on obtaining funding from agencies like NASA or ESA.  That hard fact means that the design must be optimized to keep the cost reasonable.  Managing the cost implies constraining the mass and power (because producing more power means more mass, as in larger solar panels).  The cost of putting each kilogram of  satellite mass into orbit is many thousand dollars or Euros.  Similarly, the overall size of an instrument is limited, both by the mass and fitting into a launcher (larger launchers are more expensive).  Data downlink bandwidth may also be limited (by power onboard and access to ground stations).    Reliability of long-term operation in space can only be assured by extensive (and expensive)  testing before launch, simulating launch and on-orbit conditions as accurately as possible.  In many cases, limits on some or all these parameters are dictated by the flight opportunities.  The challenge is always to maximize the scientific return within all these constraints.

\section{Examples}
Three generations of space $\gamma$-ray instruments have been flown:
\begin{enumerate}
\item The $\gamma$-ray detector on the OSO-3 satellite was a sophisticated counter telescope. It provided the first definitive measurement of high-energy cosmic $\gamma$ radiation\cite{OSO-3}.  Although it did not image the pair production events, it nevertheless showed that the Galactic plane is a bright $\gamma$-ray source.
\item Balloon payloads, then the SAS-2, COS-B, and CGRO/EGRET satellite instruments represented the second generation of instrumentation, using 1960s and 1970s technology to measure pair-production $\gamma$ rays.
\item AGILE and Fermi LAT are the current state of the art in high-energy $\gamma$-ray astrophysics, based on modern techniques used in particle physics.
\end{enumerate}

The following sections describe how the principal satellite instruments of the second and third generation dealt with the scientific and operational challenges described in previous sections.

\subsection{EGRET and Earlier Instruments}

The first $\gamma$-ray instruments with particle-tracking capability were flown on balloons in the early 1970s, confirming the bright emission from the Galactic plane \cite{Fichtel_balloon} and finding evidence for pulsed $\gamma$ rays from the Crab pulsar, e.g. \cite{Vasseur}, \cite{Browning}, \cite{Albats}.  These were followed by two small satellites:  the Second Small Astronomy Satellite (SAS-2, 1972$-$73), which mapped the Galactic emission \cite{Fichtel1975}, discovered $\gamma$-ray emission from the Vela pulsar \cite{Thompson1975}, and measured an isotropic background radiation \cite{Fichtel1978}; and the COS-B satellite (1975$-$82), which produced a catalog of high-energy $\gamma$-ray sources, 2CG \cite{Swanenburg}, including 3C273, the first extragalactic source \cite{Bignami}, as well as much greater detail on the pulsars and Galactic $\gamma$ radiation, e.g. \cite{Kanbach},\cite{Hans}, \cite{Lebrun}.  Although the instrument configurations varied, all used spark chambers as the tracking detector. Spark chambers were rugged, reliable, low-power detectors that were easily adapted to space operation.

The success of these pioneering $\gamma$-ray detectors set the stage for a major project, the Compton Gamma Ray Observatory (CGRO), a NASA mission with international partnerships.   The four instruments - Burst and Transient Source Experiment (BATSE), Oriented Scintillation Spectrometer Experiment (OSSE), Compton Telescope (COMPTEL), and Energetic Gamma Ray Experiment Telescope (EGRET) - provided a comprehensive view of the $\gamma$-ray sky from 30 keV to greater than 10 GeV.  The high-energy instrument, EGRET, is the focus of the following.

\begin{figure}[!t]
 \centering
 \includegraphics[width=9.5cm]{SPACE_Fig4a.eps}
 \includegraphics[width=6.0cm]{SPACE_Fig4b.eps}
 \caption{Left: Schematic diagram of EGRET \cite{Esposito}.  Right: composite photo of EGRET, showing the various components. }
 \label{fig:EGRET_schematic}
\end{figure}

In many respects, EGRET (Figure~\ref{fig:EGRET_schematic}) was the culmination of the experience gained from the balloon and small satellite projects, using many of the same technologies. In particular, spark chambers were used for the tracking detectors.  By 1978, when EGRET was proposed, the high-energy physics community had largely moved away from spark chambers in favor of drift chambers and multiwire proportional chambers, which offered higher spatial resolution.  For a space application, however, the low power of spark chambers became the deciding factor (the power allocated to each of the instruments on the observatory was less than 200 watts).  EGRET was a collaborative effort by NASA Goddard Space Flight Center, Stanford University, and the Max Planck Institute for Extraterrestrial Physics.

The EGRET implementation of the basic principles described above involves several subsystems and structures \cite{Kanbach_EGRET}:

\begin{itemize}
\item The converter material was a stack of 27 80 cm x 80 cm tantalum foils of 0.02 radiation length thickness, providing a reasonable detection efficiency while minimizing the effects of multiple Coulomb scattering.
\item The tracking of the $e^+$ and  $e^-$ was done by a stack of wire grid spark chambers in a sealed vessel filled with spark chamber gas (neon/argon/ethane).  28 of these were interleaved with the conversion foils, with an additional 6 chambers below with no converters, to help identify and track the particle paths.  Each chamber had 992 wires in the x direction and 992 in the y direction, where z represents the vertical, pointing direction of the instrument. Each wire threaded an individual magnetic core. The charged particles left an ionization path in the gas.  When high voltage was applied to one wire plane and the other was grounded, a spark closed the circuit, with current flowing down an x wire, across the spark to a y wire, and back down the y wire, setting the cores.  Following a trigger, the time to read out the core array and recharge the high-voltage pulsers was 110 milliseconds.
\item The triggering for the spark chamber was provided by two 4 x 4 arrays of plastic scintillator tiles, operated in coincidence with each other. The large plastic scintillator dome that surrounded the upper part of the instrument provided the anticoicidence.  The readout was photomultiplier tubes.  Because the response of plastic scintillator is fast, it was possible to use hardware logic to make a decision about the trigger in less than 1 microsecond.  In order to discriminate against unwanted upward-moving particles, a time-of-flight requirement was included, to select particles hitting the upper scintillator plane first.  The triggering tile array was also used to change the EGRET field of view dynamically, optimizing the exposure to the sky while avoiding the bright Earth limb.
\item  The energy of the electron-positron pair was measured by a sodium iodide crystal array,  8 radiation lengths thick, bonded into a monolithic detector and read out by phototubes.  In addition to the primary energy range above about 20 MeV, the energy measurement system had an independent readout in the 0.6$-$140 MeV range, used for solar flare and $\gamma$-ray burst studies.
\item The spark chambers, time-of-flight triggering system, and some of the electronics were all housed in a thin aluminum pressure vessel, filled with 1.1 atmospheres of spark chamber gas.  Because spark chamber gas gradually deteriorates in use, high-pressure tanks carried enough gas to replace the entire volume four times.
\end{itemize}

Monte Carlo simulations of EGRET provided the initial performance parameters.  The full instrument was then calibrated at accelerator facilities \cite{Thompson_calibration}.  The primary calibration was done at the Stanford Linear Accelerator Center (SLAC) using a high-energy electron beam that scattered optical laser photons to $\gamma$-ray energies (Compton scattering).  Exposures to photon energies from 15 MeV to 10 GeV and incidence angles from 0$^{\circ}$ to 40$^{\circ}$ provided a matrix of calibration points covering essentially the entire range of operation for EGRET.  A proton calibration to test for background production/detection was done at Brookhaven National Laboratory, and a follow-up $\gamma$-ray calibration was carried out at the Bates Linear Accelerator.

The experimental calibrations provided empirical input for the EGRET data analysis system.  Although the on-board triggering system was very efficient, the data sent to the ground still contained unwanted or unusable triggers.  An automated scan of the triggers rejected those with too little information or patterns inconsistent with a $\gamma$-ray pair production event, then attempted to structure the spark chamber pattern into tracks, deriving a direction and energy.  The results were reviewed by data analysts who had trained using the calibration data sets.  The basic criterion was to be consistent with a topology of a pair of tracks originating from a common point (the pair production itself), or if the energy were high enough, single straight tracks originating within (not at the edge of) the spark chamber volume.  Tests on flight data using known sources and comparison with the particle flux at different points in the CGRO orbit showed that the final data had no measurable contamination from non-$\gamma$-ray triggers \cite{Esposito}, \cite{Bertsch_calibration}, \cite{Sreekumar}.

\begin{figure}[!t]

 \CenterFloatBoxes
\begin{floatrow}
\ttabbox
{\begin{tabular}{@{}ll}
Property&Value\\
\hline
Energy Range&20 MeV $-$ $>$10 GeV\\
Peak Effective Area&1500 cm$^2$ at 500 MeV \\
Energy Resolution&15\% FWHM\\
Effective field of view&0.5 steradians\\
Timing accuracy&$<$ 100 $\mu$sec absolute\\
\end{tabular}
}
{\caption{\label{label}Some Performance Characteristics of EGRET}
}
\killfloatstyle
\ffigbox
 {\includegraphics [height = 3.5 in., angle =90] {SPACE_Fig5.eps}}
{\caption{Map of E $>$100 MeV sources in the third EGRET catalog, 3EG \cite{3EG}, shown in Galactic coordinates.  The symbol size indicates the source brightness. }
\label{fig:3EG}}
\end{floatrow}
\end{figure}

Table 1 summarizes some of the key EGRET operational parameters.  The single-photon angular resolution, or point spread function, was energy-dependent.  The point-spread function (PSF) angle $\theta_{67}$ in degrees containing 67\% of the $\gamma$ rays from a delta function source with energy E in MeV  was given by:  $\theta_{67}$ = 5.85 (E/100)$^{-0.534}$ \cite{Thompson_calibration}.

The Compton Observatory was launched on the Shuttle Atlantis in April 1991, with a planned 2-year mission.   It operated in pointing mode, with typical exposures of two to three weeks to allow adequate exposures. All the instruments were still operating when the mission finally ended in June, 2000, following the failure of a reaction wheel.  At that time, the massive (17000 kg) observatory was de-orbited into the Pacific Ocean as a safety measure.

EGRET produced the first map of the entire high-energy $\gamma$-ray sky and demonstrated the diversity of energetic phenomena detectable at these energies.  Sources ranged from solar flares just 8 light-minutes from Earth to the diffuse emission of the Milky Way to $\gamma$-ray bursts at cosmological distances.  See \cite{Thompson_review} for an overview of EGRET results.  Much of the EGRET scientific legacy is captured in the Third EGRET Catalog (3EG, \cite{3EG}), shown in Figure~\ref{fig:3EG}.  Important source classes were active galactic nuclei (mostly of the blazar class) and pulsars, with hints of other classes such as supernova remnants and binary systems containing a compact object.  Over half the 271 sources had no association with plausible $\gamma$-ray-producing astrophysical objects. Some of these were likely gas clouds that were not included in the diffuse model used for the analysis \cite{Grenier}.  Others were later found to have likely associations with known objects, e.g. \cite{3EG_blazars}.

\subsection{Fermi LAT}

By the time the Compton Observatory had completed its first all-sky survey, the early  success of that mission had led the Stanford/SLAC group to start planning a follow-on high-energy mission, taking advantage of the advances in detector technology and modeling in the years since EGRET was designed \cite{Atwood}.  That work led to the Large Area Telescope (LAT) \cite{Atwood_LAT} on the Gamma-ray Large Area Space Telescope (GLAST), renamed after launch in 2008 to Fermi Gamma-ray Space Telescope.  Fermi LAT represents an international/interagency collaboration, including NASA, the Department of Energy, and universities in the U.S. along with universities and scientific agencies in France, Italy, Sweden, and Japan.  A smaller Italian mission, Astro-rivelatore Gamma a Immagini LEggero (AGILE), uses similar technology to the LAT \cite{AGILE}.

The single most important development between the EGRET and Fermi-LAT eras was the emergence of large-area silicon strip tracking detectors.  Coupled with extremely low-power Application-Specific Integrated Circuits (ASICs), silicon strip detectors offered significant advantages over the older gas detectors:  higher spatial resolution, no pressure vessel or gas degradation, self-triggering, much faster readout, and extremely high efficiency.

Almost as significant was the dramatic increase in computing power.  Simulations at the individual detector readout level became possible, allowing not only optimization of the instrument design but also parallel development of data analysis software to reject background and extract information from the pair production particles.  Some onboard analysis could be done, giving far more flexibility in data acquisition than the largely hardware-dominated EGRET system.

\begin{figure}[!t]

 \CenterFloatBoxes
\begin{floatrow}
\ffigbox
 {\includegraphics[width=7.5cm]{SPACE_Fig6.ps}}
 {\caption{ Schematic diagram of Fermi LAT \cite{Atwood_LAT}.}   }
{ \label{fig:LAT}}
\killfloatstyle
\ttabbox
{\begin{tabular}{@{}ll}
Property&Value\\
\hline
Energy Range&20 MeV $-$ $>$300 GeV\\
Peak Effective Area&8000 cm$^2$ above 10000 MeV \\
Energy Resolution&$<$15\% FWHM\\
Effective field of view&2.4 steradians\\
Timing accuracy&$<$ 1 $\mu$sec absolute\\
\end{tabular}
}
{\caption{\label{label}Some Performance Characteristics of Fermi LAT}}
\end{floatrow}
\end{figure}

The Fermi LAT (Figure~\ref{fig:LAT}) implementation of the basic principles differs somewhat from the EGRET design, taking advantage of the new technologies available \cite{Atwood_LAT}:

\begin{itemize}
\item The tungsten converter foils are divided into two sections.  The 12 upper (front) layers are each 0.03 radiation lengths thick (to minimize Coulomb scattering effects that are important at lower energies), while four lower (back) layers have 0.18 radiation length thickness (to provide more converter for high-energy $\gamma$ rays that are less affected by scattering).
\item The trackers are 18 x-y pairs of single-sided silicon strip detectors with strip pitch of 228 $\mu$m, with the first 16 interleaved with the converter foils.  The trackers are modular, with 16 towers in a 4 x 4 array; the total number of data channels is approximately 880,000.  The tracker system self-triggers on a pattern of three consecutive x-y pairs producing a signal. Not requiring a separate time-of-flight coincidence trigger allows the LAT to be more compact, increasing its field of view, although the absence of a time-of-flight signal complicates the background rejection.
\item  The energy measurement is carried out by a calorimeter of 1536 cesium iodide logs, stacked in 8 layers with directions alternating x and y, read out by custom photodiodes. The calorimeter modules are arranged in the same 4 x 4 array of towers  as the tracker.  The hodoscopic structure allows the shape of high-energy showers to be measured, enabling measurements to higher energies than was possible with the EGRET system.
\item  Unlike the single-piece EGRET anticoincidence scintillator, the LAT system consists of 89 individual scintillator tiles, overlapped, with scintillating fibers covering seams.  EGRET was subject to self-veto, especially at high energies, when backward-moving secondary particles from electromagnetic showers hit the scintillator.  With the LAT, only tiles close to the direction of the incoming $\gamma$ ray need to be examined.
\item Although the EGRET hardware trigger was a bit faster than that of the LAT, the LAT readout is dramatically faster, with only 26 $\mu$s dead time.  This improvement permits LAT to handle much higher trigger rates.  Coupled with the much larger telemetry bandwidth available to the LAT, this high rate enables much more information to be transmitted to the ground.
\end{itemize}

The design and performance parameters for the Fermi LAT were optimized with extensive Monte Carlo simulations.   Accelerator beam tests were carried out on an engineering model \cite{Atwood2000} and a calibration unit consisting of a subset of flight-design detectors \cite{Baldini}.  The same type of simulation package used to design the instrument was used to develop automated analysis procedures for the data, eliminating the manual review that had been needed for EGRET.  The automated analysis separated the pair production events from unwanted triggers and determined the arrival direction and energy for each event.  Having an automated system has also allowed the LAT team to re-analyze data as improved knowledge of the instrument and its space environment have become available, e.g. \cite{Pass7},\cite{Pass8}.  Table 2 shows some of the key performance parameters of the Fermi LAT.   An approximation for the PSF 68\% containment angle  $\theta_{68}$ in  degrees for $\gamma$ rays with energy E in MeV converting in the front (thin-converter) section of the LAT is given by \cite{LAT_PSF}

\begin{equation}
\theta_{68}=\sqrt{(\mathrm{3.5}(E/100)^{-0.8})^2 + \mathrm{0.15}^2}
\end{equation}

\noindent Back-converting $\gamma$ rays have a PSF angle about twice as large.  At low energies, the LAT PSF is similar to that of EGRET, but the LAT PSF improves faster with increasing energy.  Current details about LAT performance parameters can be found at \url{http://www.slac.stanford.edu/exp/glast/groups/canda/lat_Performance.htm}.

The Fermi observatory has spent most of its observing time in scanning mode, with the LAT looking away from Earth.  Taking advantage of the huge LAT field of view, the typical pattern is to rock the satellite south of the orbital plane for one 96-minute orbit, then rock north for the next orbit.  In this way, LAT achieves exposure to the entire sky every 2 orbits. During passages through the high-particle-intensity South Atlantic Anomaly, triggering is disabled.

The combination of large effective area, huge field of view, and scanning mode of operation has allowed LAT to produce a $\gamma$-ray data set vastly larger than all previous satellite missions combined.  The Third Fermi LAT Catalog (3FGL, \cite{3FGL}), shown in Figure~\ref{fig:3fgl}, has more than an order of magnitude more sources than the 3EG catalog.  Discoveries have included large-scale features like the Fermi bubbles \cite{Bubbles}, new source classes (e.g. $\gamma$-ray novae \cite{novae}) and an unprecedented level of detail about known sources.  AGILE has also contributed to the growing field of high-energy $\gamma$-ray  astrophysics.  Many of the other entries in this volume discuss  the results from these satellite instruments.

\begin{figure}[!t]
 \centering
 \includegraphics[width=14.5cm]{SPACE_Fig7a.eps}
 \includegraphics[width=14.5cm]{SPACE_Fig7b.eps}
 \caption{Fermi LAT third catalog \cite{3FGL}. }
 \label{fig:3fgl}
\end{figure}

\section{Conclusion}

Satellite instrumentation for E$>$100 MeV $\gamma$-ray  astrophysics has advanced tremendously since the first detections by OSO-3.  The field now covers a broad range of topics, ranging from local phenomena in our Solar System to objects like blazars and $\gamma$-ray bursts at cosmological distances.  At the time of writing, Fermi and AGILE are both still operating well and are capable of many more years of useful observations.  There are no major technological developments on the horizon that seem capable of making the same sorts of major advances achieved in past missions.  Future satellite $\gamma$-ray projects appear likely to focus on specialized areas such as lower energies, higher angular resolution, and sensitivity to polarization.
The current generation of instruments has by no means exhausted their capabilities.  New discoveries in this energy range are still expected.

\section*{Acknowledgements}
Space missions like the ones described here involve many scientists, engineers, technicians, managers, and others.  I extend thanks to all those who have made space $\gamma$-ray astrophysics the dynamic field that it is today.  Special thanks go to Robert Hartman for valuable suggestions during the preparation of this article.

Figures 3, 4, 5, 6, and 7 are reproduced by permission of the American Astronomical Society.

redpajama_set_name: RedPajamaArXiv


text:
Ultimate guide to winning in the gaming world
James Matthew
Whether you're a seasoned gamer or just starting out, it's important to know the basics of gaming. In this guide, we take a look at the most important pieces of gaming knowledge and teach you how to win in the world of online and console games. We cover topics like strategy, tips for beginners, and how to find the right game for your skillset. If you're looking to up your game, this is the guide for you!
What is Gaming.
There are many types of gaming systems out there, and they all have their own unique strengths and weaknesses. For example, traditional board games like Monopoly or Chess can be played solo or with friends, whereas video games like Super Mario Bros. can be enjoyed by both single players and multiplayer systems.
Gaming devices such as consoles or handhelds allow gamers to access a wide variety of gaming content and challenges, making it an ideal way for people of all ages to enjoy their favorite games.
The Different Types of Gaming Systems.
There are a variety of gaming systems available on the market today, each with its own advantages and disadvantages. Here are three examples:
1) Console gaming systems: These include personal computers that are connected to the internet and used to play your favorite console video games, such as Xbox 360, Playstation 3, PC/Mac, etc. This type of gaming is convenient because you don't need any extra equipment aside from your console (which usually comes standard). However, console gaming systems can be expensive to operate (especially if you want to buy multiple copies), so it's not the best option for budget-conscious travelers.
2) Online gaming systems: These are similar to console gaming machines but they're instead connected directly to the internet and used to play classic online games like Warcraft III: The Frozen Throne or World of Warcraft. They're also often more affordable than consolegaming platforms because you don't need any additional equipment aside from your internet connection (which usually comes standard). However, onlinegaming platforms can sometimes be slow or unstable, so they're not the best choice for busy travelers who want quick and easy gameplay.
3) Mobile game platforms: These are devices that allow you to play mobile games on your phone or tablet while you travel. This type of gaming is great for people who want something different when they're traveling because it doesn't require any sitting in traffic or waiting in line for hours on end!
How to Make Money Playing Games.
There are a number of ways to make money playing games. For example, you could sell your games on eBay, Amazon, or other online platforms. Alternatively, you could start a game development company and sell game updates and new content. And if you're lucky enough to have a lot of friends who are into gaming, you could team up and start a gaming tournament.
Make Money by Selling Games.
Another way to make money playing games is by selling them online. This can be done in a number of ways, such as through an online store or marketplace, or through auctioneering. You can also sell your games directly to consumers through websites like Craigslist or Ebay.
Make Money by Playing Games for More Money.
If you want to make more money playing games than just buying them, there are several ways to do so. One option is to try playing the game for more money than it costs to purchase it. This can be done through earning rewards for completing tasks or earning points that can be redeemed for prizes in the game itself or elsewhere in the world. Additionally, some developers offer paid subscriptions that give players access to increased levels of play or special features within the game.
How to Play the Best Games.
One of the most important aspects of playing games is learning the game strategy. This guide will teach you how to play the best games, so that you can achieve the goals you set for yourself. In addition, find a gaming club or organization in your destination city to help you get started and learn more about gaming.
Find the Best Games to Play.
There are many great games to play, but it's important to find ones that fit your interests and skill level. To find these types of games, visit online gaming stores or check out online reviews to see what others have had to say about them. Additionally, join a gaming club or organization in your destination city for support and advice on which games to play and how to win.
Gaming is a great way to have fun and make some money. There are many different types of gaming systems, so you can find the perfect game for your needs. Additionally, joining a gaming club or organization can help you get more out of playing games. By learning the game strategy and finding the best games to play, you can make sure that you're able to make some serious money while enjoying yourself.


text:
Q: Is there a keyboard shortcut to put the focus on the name box in Excel 2016? I wonder if I can jump to the name box (the one above the column "A", and below the ribbons) via a keyboard shortcut.
(somewhere I've read about Alt+F3, but it doesn't work)
Thanks in advance.

A: The keyboard shortcut to focus on the name box in Excel is
Alt+F3.

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