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Q: Spring Boot - two datasources configured - how to use second datasource? I have configured two schemas from MySQL database in my Spring Boot application and have marked one datasource as Primary.
Now, my question is how can I "use" second datasource? I am using JpaRepository based approach and when I try to save something to a table which resides in second DB schema, my Spring boot application always try to find this table in first DB schema and eventually throws table does not exist error.
P.S. I have marked second DB schema in my Entity class correctly.
Below is my application.properties file (prefix has been changed to omit confidential name):
# source 1
myframework.data.sql.connections.dataSource.url=jdbc:mysql://localhost:3306/schema1?autoReconnect=true&useSSL=false&rewriteBatchedStatements=true
myframework.data.sql.connections.dataSource.user=root
myframework.data.sql.connections.dataSource.password=root
myframework.data.sql.connections.dataSource.driver-class-name=com.mysql.jdbc.Driver
myframework.data.sql.connections.dataSource.config.preferredTestQuery=select 1 from dual

# source 2
myframework.data.sql.connections.master.url=jdbc:mysql://localhost:3306/schema2?autoReconnect=true&useSSL=false&rewriteBatchedStatements=true
myframework.data.sql.connections.master.user=root
myframework.data.sql.connections.master.password=root
myframework.data.sql.connections.master.driver-class-name=com.mysql.jdbc.Driver

A: Found solution on this Blog - ScatterCode
The fix is that one has to split application configuration class into two and annotate each of the classes with what is shown below:
Config class 1:
@Configuration
@EnableTransactionManagement
@EnableConfigurationProperties({ MyServicefacadeProperties.class })
@EnableJpaRepositories(entityManagerFactoryRef = "myEntityManagerFactory", transactionManagerRef = "myTransactionManager", basePackages = {
    "com.myorg.foo" })

Config class 2:
@Configuration
@EnableTransactionManagement
@EnableJpaRepositories(entityManagerFactoryRef = "masterEntityManagerFactory", transactionManagerRef = "masterTransactionManager", basePackages = {
            "com.myorg.foo.master" })

One dataSource should reside into first config class and second one in another. Also, move the Entity class and JpaRepository interface into respective packages as indicated in annotations above.
Cheers

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Racial tensions, college partying and hookups, film festival awards, interesting camera angles and breakout performances: this dramedy has all the ingredients of an Oscar winner.
Racial tensions, college partying, film festival awards, unique camera angles and breakout performances: this dramedy has all the ingredients of an Oscar winner.
The new movie "Dear White People" tackles racial tensions in the age of Obama in a film that addresses this issue both head–on and from alternative angles. The film asks a ton of questions and then provides multiple answers to them all. Can there still be racism in a country with a black president? What should schools do about social segregation? Who does affirmative action really help? What stereotypes do people have about other races or about the proper representation of his/her own? Why is everyone obsessed with "the other"? Can black people be racist? What is the difference between racism and prejudice? All of these get played out on campus at the elite Ivy League Winchester University.
The film focuses on four black college students: Troy, Coco, Lionel and Sam. Even though all the marketing and press for the movie focuses on all four of the students, Sam really steals the show, while many other characters (both black and white) besides the core four do excellent jobs in their supporting roles. The best part is, no single character is made to be totally the righteous hero or the all–evil bigot. Even with so many characters and sub-storylines, the film still gives every character complexity in their thoughts and opinions. Sam hosts her own, very provocative campus radio show called "Dear White People," on which she addresses all the white students on campus and tells them exactly what she's thinking. She creates a petition in opposition to the university's new randomization of housing act, which threatens to break up Armstrong–Parker, the traditionally back dorm. As her movement becomes bigger and bigger, Sam and black culture on campus become the theme of the campus humor magazine's annual, outrageous, Halloween party.
Like the party, this satire is outrageous, intentionally making its audience uncomfortable in a successful effort to be provocative. Watching as a current college student, you may find yourself needing to suspend your disbelief in the less–realistic moments (the president of the university just happens to have random meetings with students, Sam may or may not have written a book, etc.). But one thing is for sure, if you thought the party in the climax scene was unrealistic, the filmmakers want you to think again. As the credits roll, the audience is confronted with pictures and news articles about parties just like the one in the film that recently happened at universities all over the country. See this movie with a friend: you're going to want to talk about it afterwards.


Place all ingredients in a food processor and process until combined thoroughly.
The mixture will look crumbly, but squeeze it in your fist to see if it adheres. If needed add a little more coconut oil or maple syrup.
Form into balls and refrigerate before serving.


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There is only one english school in Hamburg for faculty to choose from. Below are statistics and other relevant data to help analyze the state of english and english education in Hamburg, which includes english training at the english bachelors degree level.
Of the 14,350 english professionals employed in New York, 390 work in Hamburg. The number of english professionals in Hamburg has shrunk by 11% from 2006 to 2010. Overall employment in Hamburg has increased.
Salaries for english professionals in Hamburg have decreased. Hamburg english professionals made $49,170 per year, on average, in 2010. The average salary for english professionals in Hamburg was $56,853 per year, four years earlier in 2006. This decline is slower than the salary trend for all careers in Hamburg.
English professionals in Hamburg earn a median salary of $44,363 per year. The 10% of english professionals in the lowest pay bracket earn less than $26,530 per year, while those in the highest pay bracket earn approximately 201% higher salaries.
Hamburg english professionals have earnings that are lower than the salaries earned by others in related fields, on average.
Many of Hamburg's english professionals are graduates of the only accredited english school in the city.
Hamburg's english school offers one english degree and certificate program.
Approximately 3 students completed english courses in 2010.
We are in the process of collecting data for the number of english faculty, growth in the field of english academia and english faculty salaries in Hamburg. Please enter your information in the form below if you are involved in teaching english courses to students at the bachelors degree in english level. This will help us build a valuable free database resource for the benefit of current and future faculty in the field of english in Hamburg. All information you submit will be anonymous. Once you have submitted your information, you will be able to view a summary of some of the data we have collected so far.


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PA images. Brian O'Driscoll and his team-mates celebrate after the game.
# March on
Match report: Ireland show the world they're here to play
Declan Kidney's men progress after impressive win over Azzurri.
Oct 2nd 2011, 10:53 AM
MUCH LIKE THE devil, Italy thrive on chaos.
Ireland's job today was to keep it clean and simple, let talent be the deciding factor.
The final winning margin of 36-6 was fully deserved, as they not only secured a quarter final spot, but put in the most clinical performance of the season by any European side.
Where the win over Australia was all emotion and desire, this one was mean and focused and professional, a thorough annihilation of a decent Italian side.
The opening exchanges were messy, Sean O'Brien and Quintin Geldenhuys knocking on when under no pressure, and Tommy Bowe throwing a no-look pass that was never on, but Ireland always looked the more threatening in open play, changing the point of attack at every opportunity, forwards and backs interlinking well throughout.
It didn't lead to any tries for the first 40 minutes, three O'Gara penalties giving them a 9-6 lead going into the break, but the blueprint for success was there.
There was a different level of intent in the second period, however, O'Brien and Ferris going from snarl to roar, both carrying three times in the first five minutes, blasting through inside shoulders every time. Italy were bruised and pulpy, ripe for squashing . A smart outside arc by Tommy Bowe, followed by a simple but brilliant inside pass to the supporting O'Driscoll did the damage, opening it out to a 19-6 lead after 47 minutes.
That ignited Ireland's best period of the game, Darcy, O'Brien and O'Connell gaining ground at will, and as the Italian defence began to wilt Ferris again showed there's brains to go with all that brawn, neatly putting Keith Earls in for what was effectively the deciding score.
Things got scrappy for a period after that as scrums collapsed and the Italians got tetchy, but the final bell saw Andrew Trimble show great composure in tight space to put Earls over for his second of the night, sending a huge Irish crowd into raptures.
If Ireland are to go beyond the quarters, they will need to play well for longer periods, but there was an encouraging collective understanding of where the space was and who to put into that space. The Italians had plenty of possession and grunt, but the guile only came from one quarter, and the stand-out performers all wore green.
O'Gara missed only one kick at goal, Murray made two breaks and passed well, Bowe and Earls were sharp as tacks, and the pack once again showed they have the fire and ice required at this level.
This was more than a win, it was cold-hearted destruction, deliberate and tough, and it has sent a message out to the rest of the teams in the tournament – Ireland are here to play.
As it happened: Ireland v Italy
Simon Hick
@poshboyhick
IRFU MARCH ON NEW ZEALAND RUGBY WORLD CUP RWC2011 IRELAND ITALY
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Shares of the motorcycle maker fell on macroeconomic issues and a weak earnings report.
Harley-Davidson has been one of the victims of President Trump's trade war: The European Union slapped tariffs on its motorcycles, and investors have continued to worry about trade tensions with China, which has also punished the classic American motorcycle maker with tariffs.
Harley's troubles continued when the company reported third-quarter earnings, pushing the stock down 2% as domestic sales continued to disappoint. Retail motorcycle sales fell 13.3% to 36.2 million vehicles in the U.S., and global sales were down 8% to 59.2 million. That slide has been ongoing; millennials have not been buying motorcycles at the same rates as older generations, so Harley finds itself with an aging customer base, a problem for which there is no easy solution.
Revenue jumped 16.8% to $1.12 billion in the quarter, helped by the timing of shipments, and adjusted earnings per share surged to $0.78. Both results beat estimates, but were overshadowed by the domestic weakness. CEO Matt Levatich said: "As we manage our business with resilience in a challenging time in our history, we are leveraging our strengths for a more promising road ahead. We are investing to build the next generation of Harley-Davidson riders and we are optimizing our business to drive profitability and cash flow."
In its guidance, the manufacturer said it expected full-year sales to be at the low end of its previous guidance of 231,000 to 236,000 vehicles. Year to date, the stock is now down 20%, succumbing to the same challenges as other motorcycle manufacturers. As long as motorcycle sales continue to slide, the stock should remain pressured.


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rotisserieduckdotcom
Baseball Analysis & Baseball Cards
A Minor Diversion
The real difficulty is explaining how much fun it is to be a baseball junkie. For the uninitiated, the game holds endless facts and stories about teams, seasons, games, players and outcomes. The history of the game is what makes it all come together. Who could know that a young Pitcher named Babe Ruth would eventually set a record for hitting Home Runs? Who could imagine that a skinny High School basketball player would turn out to be a Hall of Famer named Sandy Koufax…and did you know that he was born Sanford Braun?
You can never run out of stories when it comes to our national pastime. I was reminded of this vividly when a collection of minor league baseball cards recently came across my desk. One of the team sets featured the 1988 Las Vegas Stars, the AAA affiliate of the San Diego Padres. The team finished the Pacific Coast League season with a record of 74-66 but as with all teams, there are 25 stories beneath the surface. Let's take a look behind the curtain at the 25 individuals in this beautiful, black-bordered card set.
> #1, Joe Bitker P – The workhorse of the rotation, he pitched 178 innings with a 3.58 ERA and a record of 8-10…he was 11-9 the previous season for the Stars. He pitched briefly in the majors in 1990 & '91, appearing in only 15 games. His lifetime big league record was 1-0…undefeated!
> #2, Keith Comstock P – A veteran at age 32, he was the Closer and had 5 Wins & 17 Saves. His career included two seasons in Japan and stints with four big league clubs. The left-hander had a lifetime major-league record of 10-7.
> #3, Greg Harris P – One of the Padres top prospects, he was 9-5 at age 24 and made his big league debut that September. Pitched in eight seasons as a major-leaguer with a lifetime record of 45-64 and a 3.98 ERA.
> #4, Joel McKeon P – Was 2-5 for the Stars with a 5.96 ERA. He had pitched for the White Sox in 1986 & '87 but never made it back to the majors.
> #5, Pete Roberts P – Started 13 games and had a record of 4-6. Pitched three more years at the high levels of the minors but never made a big league appearance.
> #6, Todd Simmons P – Had a true "vulture" campaign as he pitched 54 games in relief and complied a record of 12-5. Completed one more minor league season and was out of baseball at age 25.
> #7, Ed Vosberg P – A very useful swing-man, he started 11 games and pitched another 34 in relief. Finished with a record of 11-7 and posted 2 Saves. His baseball career spanned from 1983-2007 and he pitched in 10 big league seasons before retiring at age 45. The prototypical situational left-hander, he won a total of 10 games in the majors and was part of the 1997 World Series champion Marlins.
> #8, Kevin Towers P – A familiar name that was recently in the news as he passed away at age 56 just last week. 1988 was essentially his last season as a player but he later became a famous front office executive. After starting as a scout for the Padres in 1990, he eventually became their GM, serving in that capacity from 1995-2009. From 2011-2014, he was the GM of the Diamondbacks.
> #9, Joe Lynch P – Was 6-6 with 8 Saves out of the bullpen and had an impressive 3.27 ERA. Pitched two more seasons for the Stars and retired at age 27.
> #10, Shane Mack OF – Got 267 AB's with the Padres in 1987 and got back up to the big club again in '88. His real MLB success came during his stint with the Twins from 1990-1994 where he hit over .300 in four of the five seasons. Played in Japan in 1995 & '96 before coming back to the majors for a few more years. He was a lifetime .299 hitter with a .821 OPS in nine big-league campaigns.
> #11, Thomas Howard OF – Played with the Stars in both '88 & '89 before making his big-league debut with the Padres in 1990. Ended up with over 2,600 big league AB's over 11 seasons. Also played for the Indians, Reds, Astros, Dodgers & Cardinals.
> #12, Jerald Clark OF – Hit .301 in 408 AB's for the Stars. Ended up playing parts of seven seasons in "The Show" with a lifetime BA of .257. His Brother Phil played for three teams in the 90's and hit .276.
> #13, Randy Byers OF – A .267 hitter in 100 games for the Stars, he only had 26 major league AB's and was out of baseball before turning 24.
> #14, Bip Roberts 2B – Hit .353 with 29 SB's and was on his way to the majors. One of the quickest players in the NL during the early 90's, he had 46 SB's for the Padres in '90 and 44 for the Reds in '92. Leon (his real name) played 12 years with over 1,200 Hits and a .294 BA. Made over $17 Million during his big league career.
> #15, Brad Pounders 1B – A productive bat in '88 with 14 HR's & 74 RBI's but it was his last professional season at age 24. His Son Brooks did make the major leagues and pitched for the Royals in 2016 and the Angels in '17.
> #16, Rob Nelson 1B – The power hitter in the middle of the line-up for the Stars, he hit 23 HR's with 77 RBI's in 388 AB's. Ended up with only 152 major league AB's and hit .178.
> #17, Gary Green SS – Had over 300 AB's and didn't hit a HR. Eventually accumulated 180 AB's in the big leagues and didn't hit a homer there either. His Dad Fred pitched in the majors during the early 60's and was a member of the 1960 World Series champion Pirates.
> #18, Joey Cora 2B – This diminutive infielder hit .296 for the Stars and only struck out 19 times in 460 AB's. Spent 11 years in the majors and had over 1,000 Hits with a .277 lifetime BA. His Brother Alex played 14 seasons and is the new Manager of the Red Sox.
> #19, Mike Brumley SS – Hit .315 and swiped 41 bases for the Stars. A switch-hitter, he played parts of eight seasons in the majors before retiring in 1996. His Dad (also named Mike) was a Catcher for the Washington Senators from 1964-66.
> #20, Roberto Alomar, SS/2B – Even though he was only 20 years old, the talent level was obvious and he got called up to the Padres after only nine games in Las Vegas. His rookie season gave a glimpse of what was to come with a .709 OPS & 24 SB's. One of the best fielding 2B in the history of the game (he won 10 Gold Gloves), he was inducted into Cooperstown in 2011. His Dad & Brother (both named Sandy) were also major leaguers.
> #21, Bruce Bochy C – At the other end of the spectrum from the young players, this was his last season as an active player after playing parts of nine years in the majors. The epitome of a back-up Catcher, his lifetime BA was .239. He managed in the minor leagues for the next four years and became the skipper of the Padres in 1995 and stayed for 12 years including a World Series appearance in 1998. In 2007, he took over the helm with the Giants and three world championships later, he is one of the most respected leaders in the game. After 22 seasons and almost 1,800 Wins, he may be on track to Cooperstown someday.
> #22, Sandy Alomar, Jr. C – A .297 BA with 16 HR's put him on the radar at age 22. Became the starting Catcher for the Indians in 1990 and made six All-Star teams in his career.
> #23, Tom Brassil IF – This was his 7th minor league season and despite hitting .311, he called it quits at age 28.
> #24, Steve Smith Manager – A minor league infielder form 1976-82, he never made the majors. He managed in the minors for 12 years, half of them at the AAA level.
> #25, Sonny Siebert Coach – An outstanding major-league Pitcher in the 60's & 70's, he won 130 big league games with a lifetime ERA of 3.21. Won 16 games three times and made two AL All-Star teams.
Lots of baseball history from a minor-league team that played 30 years ago. One, and possibly two, Hall of Famers, multiple All-Stars and some baseball heritage of families that played the game. If you think this team is the exception to the rule, think about this…we could have chosen the 1988 Richmond Braves and talked about the cards of John Smoltz, David Justice, Lonnie Smith, Jeff Blauser & Leo Mazzone.
As always, the history of the game is what makes it all come together.
Posted on February 8, 2018 Author cflduck
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Lawyers for the WikiLeaks publisher want the OAS independent body to keep Assange from being sent to a courtroom in the U.S. and to end his isolation.
The Guardian has claimed Paul Manafort visited Julian Assange at the Ecuador embassy. John Pilger visited Assange and tells CN's Joe Lauria Assange strongly denied any such meeting.
Consortium News broadcast the 9th Online Vigil for Julian Assange Friday night. Among the special guests were journalist and filmmaker John Pilger, who visited Assange at the Ecuador embassy in London. Watch the replay here.
While media focused on Julian Assange's cat rather than his continuing arbitrary detention, evidence shows Britain worked hard to force his extradition to Sweden where Assange feared he'd be turned over to the U.S., as Stefania Maurizi explains.
Watch live an emergency meeting being held on new threats to Julian Assange.
An attempt was made on Oct. 29 to break into the Ecuadorian embassy, where security has been removed and apparently new surveillance devices installed, reports Joe Lauria.
New threats to the safety of Julian Assange, to be disclosed shortly by Consortium News, have prompted an emergency meeting of his supporters.


We are currently looking for an Administrator to work for one of the largest facilities management companies in the UK, working at the headquarters of one of their flagship sites in London. The role will include day to day administration tasks, working closely with the office managers, chasing documentations, being involved with the planning of projects and answering call and emails.
- The capacity to think ahead, plan and prioritise own workload.
- The ability to work under pressure and meet deadlines.
- The ability to work as part of a team.
- The ability to build professional working relationships with internal/external stakeholders.
- Work safely in accordance with the company's current health and safety policy and procedures.
- FM Industry specific knowledge.
You will also be asked to undertake projects and any other duties, which reasonably fall within the scope of the position, and you will also need to demonstrate capacity to develop within the role and take responsibility for driving own professional development.


Join us for a sustainable dining experience at Charcoal Lane and find out more about what is happening in our local area to ensure a sustainable food future.The world is becoming increasingly aware of the need for sustainable production and consumption. Addressed in both Sustainable Development Goal 2 – Zero Hunger and Goal 12 – Responsible Consumption and Production, growers, suppliers, restaurants and home cooks are all seeking to play a part in minimising the impacts of climate change and meeting sustainable waste management challenges.
Marcus Godhino is CEO of social enterprise FareShare, which rescues surplus food and cooks 5,000 free, nutritious meals for Victorians doing it tough. Marcus was previously director of Environment Victoria, and also managed fundraising and partnerships at the Australian Conservation Foundation.
After studying a Bachelor of Food and Nutrition Science and Master of Dietetics, Em Massey joined Deakin's Campus Services Division as a graduate project officer working on the implementation of the Deakin Food Charter's five pillars: healthy, sustainable, informed, easy and balanced. She is passionate about food and sustainability and excited by the innovation and newness of her role. Working closely with the hospitality team, Em has been able to apply her nutrition knowledge in a meaningful – if somewhat unconventional – way.
Jane Kou is the Founder & CEO of Bring Me Home, an online marketplace that connects people to food retailers with discounted surplus food to sell.
Jane previously worked with a similar venture from Europe that has now saved over 3.6 million meals from going to waste. She's also a graduate from Melbourne Business School, and a semi-finalist of the Victorian Young Achiever Awards.
Greg Hampton is the Executive Chef at Charcoal Lane. He has more than 25 years' experience in kitchens from Cairns to Healesville. Greg is passionate about using and growing native Australian ingredients, fusing them with contemporary cooking techniques to create a flavoursome and balanced menu. A qualified horticulturalist and teacher, Greg has been teaching young chefs since 2009.
Charcoal Lane is a Mission Australia social enterprise restaurant that provides guidance and opportunity to young people, many of whom are Aboriginal, and in need of a fresh start in life.


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Jimmy Fallon and Justin Timberlake are BACK on SNL! [VIDEO]
Everytime Justin & Jimmy get together - it's AWESOME! Their chemistry works, and they crack each other up - which is always funny to watch. They have some of the most memorable skits ever on SNL - and that says a lot.
Hey, it's Trent, Jimmy and Justin are 2 stars who who are so natural together. I've been a fan from the start. Whether it's SNL, Jimmy's show, MTV or anywhere - whenever they are doing anything together - we are there.
This story has all the details on their triumphant return to Saturday Night Live. Fallon and Justin Return To SNL!
#Hashtag Jimmy and Justin is from Jimmy's show and is really funny - it's how Twitter would sound if that's how we talked.
Filed Under: Jimmy Fallon, Justin Timberlake, Saturday Night Live, Trent Marshall
Categories: Articles, Videos


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Home → News → Who Heals Who?
Who Heals Who?
We are always looking to receive new groups and individuals to visit us and share in the incredible work of Shoulder to Shoulder. Principle among the reasons for this is that people are the primary resource for development work. Shoulder to Shoulder is built upon the commitment of so many who develop relationships with the people of Southern Intibucá. But the more selfish reason for looking for new individuals and groups is that we have such a great time being their hosts. Generally, it takes us a lot of work to develop relationships with universities and groups to bring them to Honduras. But sometimes our opportunities just seem to fall out of the sky into our laps.
Sometime back in the Spring we got an email from an undergraduate student, Nava, at Duke University. The group, Project HEAL (Health Education and Awareness in Latin America), had been coming to Honduras annually with another NGO. It wasn't going to work this year, and Nava was a little desperate to find another NGO to host them. We, of course were ecstatic, and even though we had something to learn about what they intended to do, and even though they were coming at a very busy time of our year, we immediately said yes. We figured we'd work out the details as we went along.
Five students, Nava, Noelle, Dahlia, Judy, and Lissa, would come to Camasca for five weeks to conduct four separate research projects on personal and community health issues. It would be during July and early August when Laura and I would be away for a time in the US; MAHEC would be here for two weeks in a forty person brigade; two MSW students from the University of Chicago would be doing an internship here. Then, to top it off, the surprise component would be that we would have to replace our brigade coordinator. Could we pull this off? Could we give Project HEAL a meaningful experience while we had so many other irons in the fire? Of course we could, and we did.
At the Urbana with Nava
They wanted to live with families while here to get more of a feel for life in Camasca. We've done a little of this with volunteers, but finding homes for five students for five weeks was a big challenge. We contacted the teachers at the local primary school, the Urbana, who have been looking for ways to partner with Shoulder to Shoulder. Three teachers agreed to take the five students. There was a little bit of a catch, however. The Urbana wanted the students to teach English to the students while they were here. That wasn't part of the project portfolio that Nava had given us. But when we approached him with the proposal, he graciously agreed. The students had never taught before. They had some anxiety about it when we picked them up in San Pedro Sula. But we had a feeling they might find some magic among the children.
They busied themselves with their four projects: Teen Pregnancy and Relational Dynamics in Adolescents; Self-Esteem for Adolescents; Cervical Cancer Attitudes, Awareness, Prevention and Treatment; and Trash Disposal and Related Attitudes/Behaviors. They visited families in the town center and among our smaller communities, doing interviews and conducting focus groups. They gathered their data, analyzed it, and put together some community trainings. They returned to the families and groups, shared their results, and taught about healthy practices. They did great work, and they will share with Shoulder to Shoulder the reports on their topics. We're certain these will become valuable tools as we continue the work they invested in and prepare for their return next year.
A Focus Group
I guess we could say they lived up to their project name and this was a 'healing' event. But we have a feeling that the really impactful moments of their time with us happened beyond their diligent work in a less anticipated way.
We planned a debriefing with the group on the day before they were scheduled to leave Camasca. Their visit to our home happened immediately following their going away celebration at the Urbana School with the teachers and the students. We couldn't start the debriefing right away because the five Duke students all arrived at our house in tears. The children, the teachers, and the families with whom they stayed, all expressed their affection for them and how much they would miss them. The kids had come so close to them — and they so close to the kids — that they had indeed become part of this community. The families now had adopted a son and four daughters, new brother and sisters, to the point that one of the Duke students was speaking to us of her cousin when we realized that it was a cousin of the family with whom she was staying. Their study was very important and meaningful, and yet the memories impressed on their hearts may have little to do with the particulars of their service. Their memories will forever include hiking up mountains, attending a rodeo during the town's fair, taking a trip to the hot baths of Gracias, Lempira, being cared for by a second mother when suffering a stomach virus, and most especially the joyous smiles of children who are so welcoming of new friends.
The Women of Project HEAL in Camasca
I suppose we often consider 'healing' a clinical response to persons who present themselves in need. We heal others when we diagnose their need and prescribe and initiate a treatment. But healing and finding health is so much more. It seems that these Duke students have taught and learned that healing is about meeting and being met, and ultimately loving and being loved.
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Nava, Noelle, Dahlia, Judy, and Lissa — you all have homes here. We look forward to your return.
On August 26, 2017 / News
The Circus Comes to Town
Here is Half a Sandwich


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Q: Building a MySQL database that can take an infinite number of fields I am building a MySQL-driven website that will analyze customer surveys distributed by a variety of clients. Generally, these surveys are structured fairly consistently, and most of our clients' data can be reduced to the same normalized database structure.
However, every client inevitably ends up including highly specific demographic questions for their customers that are irrelevant to every other one of our clients. For instance, although all of our clients will ask about customer satisfaction, only our auto clients will ask whether the customers know how to drive manual transmissions.
Up to now, I have been adding columns to a respondents table for all general demographic information, with a lot of default null's mixed in. However, as we add more clients, it's clear that this will end up with a massive number of columns which are almost always null.
Is there a way to do this consistently? I would rather keep as much of the standardized data as possible in the respondents table since our import script is already written for that table. One thought of mine is to build a respondent_supplemental_demographic_info table that has the columns response_id, demographic_field, demographic_value (so the manual transmissions example might become: 'ID999', 'can_drive_manual_indicator', true). This could hold an infinite number of demographic_fields, but would be incredible painful to work with from both a processing and programming perspective. Any ideas?

A: Do not fall for a table with key-value pairs (field id, field value) as that is inefficient.
In your case I would create a table per customer. And metadata tables (in a separate DB) describing these tables. With these metadata you can generate SQL etcetera. That is definitely superior too having many null columns. Or copied, adapted scripts. It requires a bit of programming, where an application uses the metadata to generate SQL, collect the data (without customer specific semantic knowledge) and generate reports.

A: Your solution to this problem is called entity-attribute-value (EAV).  This "unpivots" columns so they are rows in a table and then you tie them together into a single view.
EAV structures are a bit tricky to learn how to deal with.  They require many more joins or aggregations to get a single view out.  Also, the types of the values becomes challenging.  Generally there is one value column, so everything is stored as a string.  You can, of course, have a type column with different types.
They also take up more space, because the entity id is repeated on each row (I think that is the response_id in your case).
Although not idea in all situations, they are appropriate in a situation such as you describe.  You are adding attributes indefinitely.  You will quickly run over the maximum number of columns allowed in a single table (typically between 1,000 and 4,000 depending on the database).  You can also keep track of each value in each column separately -- if they are added at different times, for instance, you can keep a time stamp on when they go in.
Another alternative is to maintain a separate table for each client, and then use some other process to combine the data into a common data structure.


Quorum Information Technologies Inc. (TSX VENTURE:QIS) ("Quorum" or the "Corporation") is pleased to announce that, effective December 9, 2016, Jon Hook has been appointed a director of the Corporation.
Mr. Hook has over seven years of equity investment experience, first working at the Teacher Retirement System of Texas (TRS) for five years covering Software & Services, and at Voss Capital LLC for the last two and a half years. Prior to TRS, he worked for over three years at EMR software provider Epic Systems. Mr. Hook obtained his MBA from Rice University and holds the Chartered Financial Analyst (CFA) designation.
"This is an exciting time in Quorum's history and I am delighted to join the board. The ongoing adoption of Quorum's DMS by auto dealerships and the strong execution by the management team has been impressive. I am optimistic about the promising strategic opportunities for Quorum and look forward to working with the board to help the company realize its full potential and maximize shareholder value."
Quorum is a North American company focused on developing, marketing, implementing and supporting its XSellerator product for GM, Ford, Chrysler, Toyota, Hyundai, Kia, Nissan, Subaru, NAPA and Bumper to Bumper franchised dealership customers as well as other franchised, independent and some non-automotive dealerships. XSellerator is a dealership and customer management software product that automates, integrates and streamlines every process across departments in a dealership. One of the select North American suppliers under General Motors' DTAP program, Quorum is also one of largest DMS providers for GM's Canadian dealerships with 25% of the market. Quorum is a Microsoft Partner in both Canada and the United States. Quorum Information Technologies Inc. is traded on the Toronto Venture Exchange (TSX-V) under the symbol QIS and in 2016 was selected to the TSX Venture 50®, an annual ranking of the strongest performing companies on the TSX Venture Exchange. For additional information please go to www.QuorumDMS.com.


text:
The choice of Paris
110×74 mm, X6/8, 1995, op. # 58
owner (customer): P. Labuhn
The Judgement of Paris is a story from Greek mythology, which was one of the events that led up to the Trojan War and (in slightly later versions of the story) to the foundation of Rome.
It is recounted that Zeus held a banquet in celebration of the marriage of Peleus and Thetis (parents of Achilles). However, Eris, goddess of discord, was uninvited. Angered by this snub, Eris arrived at the celebration, where she threw a golden apple (the Apple of Discord) into the proceedings, upon which was the inscription "for the fairest one".
Three goddesses claimed the apple: Hera, Athena and Aphrodite. They asked Zeus to judge which of them was fairest, and eventually Zeus, reluctant to favour any claim himself, declared that Paris, a Phrygian mortal, would judge their cases, for he had recently shown his exemplary fairness in a contest in which Ares in bull form had bested Paris's own prize bull, and the shepherd-prince had unhesitatingly awarded the prize to the god
Clown with books


text:
South Carolina FYI
Santee Cooper Class-Action Lawsuit Settled – Here's What That Means For You
Submit Your Thoughts
In the ongoing events that surround Santee Cooper and the V.C. Summer scandal, a $520 million settlement has been made in the case of Jessica Cook. However, the settlement amount, which was already just a slither of the debt pie Santee Cooper has racked up, came out to an even lesser amount of $300 million, to be made in two payments, by the time all legal fees were paid.
The class-action lawsuit, led by Jessica Cook, was filed in 2017 over the failed V.C. Summer project and the billions of dollars wasted and being passed onto all of the utility's direct-serve and electric cooperative customers.
The settlement also includes a 4-year "rate freeze," leading many to believe that efforts to sell Santee Cooper could come to a halt. However, the debt that customers are already paying for is still being paid through their power bill, essentially paying themselves for the rate freeze. Additionally, as previously stated, the settlement amount is just a small fraction of the total debt that will eventually have to be paid off.
In the larger scheme of things, the state-owned energy company is still billions of dollars in debt, due to the V.C. Summer, failed projects, and other ventures. So, while the Cook case is a win in the eyes of some, it does little to fix all of the outstanding issues surrounding Santee Cooper or give customers any answers to the rest of the debt that is owed or the debt they're already paying for.
More news has just recently been released that the company is paying $1.1 Million to former Santee Cooper lawyer, Mike Baxley. Mr. Baxley served on the Santee Cooper general counsel and was recently laid off in efforts to cut costs. However, he was sent on his way with $495,000 and will receive an additional pension over the next 15 years. Baxley was also given additional compensation in return to agreeing not to sue the company and was added to the list of former executives who left with a golden parachute being paid by customers.
Giving large payouts is business as usual for Santee Cooper who paid gave golden parachutes to outgoing executives associated with the V.C. Summer debacle. However, what does this mean for ratepayers in the future? The company continues to shovel money into paying out their executives while the 4-year "freeze-rate" does little for Santee Cooper's direct serve and coop customers since they continue to pay for the debt as it piles up. The only real way to protect Santee's customers is to sell Santee Cooper to an IOU that will have proper oversight and eliminate the debt otherwise there is no question that rates will skyrocket at the end of the rate-freeze time period.
© 2021 South Carolina FYI. All Rights Reserved.
Santee Cooper


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

In August of 1999, the newly-launched \emph{Chandra} X-ray observatory observed the distant ($z=0.651$) quasar PKS~0637$-$752, during the orbital checkout and activation phase of the mission \citep{chartas2000,schwartz2000}, unexpectedly discovering X-ray emission from the resolved kpc-scale jet. Over the intervening years, dozens more X-ray bright jets have been discovered in which, as in PKS~0637$-$752, the X-ray emission has a hard spectrum and high flux level which clearly indicates a second emission component from the radio-optical synchrotron emission. The nature of this X-ray emission, while at some points thought understood, has had no clear identification for nearly 20 years. The few possible mechanisms imply vastly different physical conditions in the jet and total energy budgets.

Shortly after the original discovery of PKS~0637$-$752, \cite{tav00} and \cite{cel01} independently suggested that the X-ray emission could be explained by inverse-Compton upscattering of the Cosmic Microwave Background (IC/CMB). This explanation was originally considered and discarded in the discovery papers by \cite{chartas2000} and \cite{schwartz2000}; those authors assumed \citep[as is consistent with population observations generally, e.g.][]{arshakian2004} that the jet would not remain highly relativistic at 100 kpc or more from the central engine. Under only mildly relativistic conditions it is impossible to reproduce the high X-ray flux level with IC/CMB without unreasonable (many orders of magnitude) deviations from equipartition. However, \cite{tav00} found that by taking the large-scale jet to be very well aligned ($\theta<6^\circ$) and highly relativistic ($\Gamma>18$), the IC/CMB emission could be Doppler-boosted enough to match the X-ray observations, though at a cost of requiring a jet power 10 times the Eddington value. Many other jets with a second (hard) spectral component emerging in the X-rays have been modeled as cases of IC/CMB \citep[e.g.,][]{sambruna2002, sambruna2004, marshall2005, jorstad2006, tavecchio2007, marshall2011, perlman2011, kharb2012, stanley2015}. The vast majority of these jets were in sources identified as quasars, i.e., aligned counterparts of FR II radio galaxies, which are typically more powerful than FR I radio galaxies or BL Lacs (their well-aligned blazar counterparts). OJ~287 is a notable example as an FR~I \citep{marscher2011}.

While IC/CMB has been the most popular explanation for the hard X-ray emission in resolved jets, it has never been positively confirmed as the correct one. A few years before the launch of \emph{Fermi}, in a clear-sighted review of the state of the case, \cite{hardcastle2006} noted the many problems for the IC/CMB model, including the inconsistency of the highly relativistic jet speeds on hundreds-of-kpc scales with population statistics, the problem of X-ray/radio knot offsets and fine-tuning of the required minimum electron Lorentz factor. As an alternative, he suggested that a second-synchrotron model (i.e., emission from a heterogeneous rather than `one zone' model) be reconsidered. A few other authors have also preferred a second synchrotron component for some cases \citep{dermer_atoyan,miller2006}.
The difficulty up to this point was that it was not possible to use spectral energy distribution (SED) modeling of radio to X-ray data to distinguish the two scenarios. Even apparent discrepancies between radio and X-ray spectral indices can be accommodated. The spectral indices, particularly in the X-rays, are rarely well-constrained. In addition they trace very different particle populations under the IC/CMB model, with the X-ray producing electrons having a lower particle Lorentz factor ($\gamma$) by a factor of 10 or more.

\cite{geo06} noted that the IC/CMB model for the X-ray emission implies a very high level of gamma-ray emission which generally peaks at or near the \emph{Fermi}/LAT (then GLAST) band, and that the level of this emission is also completely predicted by the radio-optical spectral shape and the level of the X-ray emission. With a well-sampled radio-optical synchrotron SED, there is no freedom about the level of gamma-ray emission \citep[see also][]{meyer17}. Since the launch of \emph{Fermi} in 2008, we have been looking for this steady gamma-ray emission from second-component X-ray jets. Up until now we have not found any evidence for it, ruling out the IC/CMB model in dozens of sources (\citealt{meyer14,meyer15,meyer17,breiding2017,breiding2018_thesis}; Breiding et al., 2019, in prep.).

 In this paper we report the first detection of a low-state gamma-ray spectrum with the Fermi/LAT which is consistent with the IC/CMB predictions based on the assumption that the X-ray emission is entirely due to IC/CMB. The two sources are considerably different from one another in terms of jet power; OJ~287 is a low-power BL Lac object while \pfs is a powerful quasar.  After presenting the observations we will discuss the likely reasons that these jets are atypical compared to the majority of X-ray jets where the X-rays are not dominated by IC/CMB.

In this paper we assume the current standard $\Lambda$CDM cosmology with Hubble constant $H_0$=73~km~s$^{-1}$~Mpc$^{-1}$, $\Omega_M$= 0.27, and $\Omega_\Lambda$=0.73. At the distance of OJ~287 ($z$ = 0.306) 1$''$ corresponds to a projected distance of 4.36 kpc, while for \pfs ($z=0.36$) it corresponds to 4.87 kpc.

\begin{figure*}[t]
    \centering
    \includegraphics[width=6.5in]{FIGURE1.eps}
    \caption{Chandra X-ray imaging of OJ~287 and \pfs with radio contours overlaid. OJ 287 is in North-up orientation while \pfs has been rotated for comparison. The (0.4-8 keV) \emph{Chandra}/ACIS observations are from Observation IDs 9182 and 11432; they have been reprocessed using CIAO ver. 4.11 and have been rebinned to 1/5 native scale. The radio contours shown on the OJ~287 image are from L-band A-configuration VLA observation AC108 (clean beam size 1.69$''$ $\times$ 1.59$''$)  while \pfs are from C-band A-configuration VLA observation AO070 (clean beam 0.51$''$ $\times$ 0.39$''$).     }
    \label{fig:X-ray}
\end{figure*}

\section{Data Sources and Methods}
\subsection{VLA and ALMA}

For OJ~287, the radio fluxes for the entire large-scale jet at 1.4 GHz, 4.8 GHz, and 8.6 GHz were taken from \cite{marscher2011}. This source has also been utilized as a calibrator source for ALMA observations; we analyzed relatively deep Band 3 observations taken from project 2016.1.00406.S where OJ 287 served as phase calibrator, but the jet was not detected -- likely because of dynamic range limitations given the very bright core (5.5 Jy at 100 GHz).

For \pf, we analyzed historical VLA observations at L and C band in A-configuration from project codes AH938 and AO070, respectively. The data were calibrated using standard procedures in CASA version 5.3.0; as the source is very bright \pf~was used as its own phase calibrator. Several rounds of phase-only (non-cumulative) and a final amplitude and phase self-calibration were applied to the data after successive deconvolutions with CLEAN as is standard practice for bright compact sources. The final RMS of these images were 4.5 $\times$ 10$^{-4}$~Jy and 1.9 $\times$ 10$^{-4}$~Jy, with synthesized beam sizes of 1.56$''$ $\times$ 1.15$''$ and 0.51$''$ $\times$ 0.39$''$, respectively.

\pfs has also been observed by ALMA; we reduced archival band 4, 6, and 7 observations from project 2016.1.00116.S. The data were initially processed using the `scriptForPI.py' script with CASA in pipeline mode. In all cases, after initial imaging we applied 1-2 rounds of phase-only self-calibration before a final round of amplitude and phase self-calibration. The final RMS of these images was 7.3 $\times$ 10$^{-5}$~Jy, 1.0 $\times$ 10$^{-4}$~Jy and 1.6 $\times$ 10$^{-4}$~Jy with synthesized beam sizes of  2.49$''$ $\times$ 1.72$''$, 1.82$''$ $\times$ 1.36$''$, and 1.20$''$ $\times$ 0.93$''$, respectively.

For all radio imaging analyzed here we produced `core-subtracted' images in order to better isolate the total flux from the extended jets. To do so we used CLEAN to populate the `model' column of the post-self-calibration CASA MS file with components only at the location of the core and then subtracted these from the visibility data using the CASA task \texttt{uvsub}. We then ran a final round of CLEAN on the now-subtracted MS file to produce the image without core emission.

\subsection{HST and Chandra}
Both jets have been observed in the optical by HST, with only upper limits to the jet emission as reported by previous authors \citep{marscher2011,sambruna2004}, which we have included in our SEDs.

In the X-rays, OJ~287 has been observed once by \emph{Chandra} in 2007 December and the flux of the entire jet is reported in \cite{marscher2011} as 3.06 $\pm$ 0.09 $\times$ 10$^{-2}$ cts s$^{-1}$ from 0.2$-$6~keV. Using their measured spectral index for the entire jet of $\alpha$ = 0.61 $\pm$ 0.06 we have converted this to 10.4 $\pm$ 0.3~nJy at 1~keV.

\emph{Chandra} observations of \pfs were first reported by \cite{sambruna2004} based on a 9~ks observation from 2001 March. We re-analyzed a deeper 45~ks ACIS-S observation from (OBSID: 11432), which was taken on 2010 April 5 using the FAINT telemetry mode. The analysis was conducted using CIAO 4.11. After standard reprocessing using CALDB 4.8.2, we screened the data for background flares (there were none) and extracted the data from 0.4-8 keV with a final exposure time of 43.38~ks.

\begin{figure*}[t]
    \centering
    \includegraphics[width=7in]{Figure2.eps}
    \caption{Results of the progressive binning \emph{Fermi}/LAT analysis for OJ~287 (left) and \pf, (right). We have plotted the $\nu F_{\nu}$ flux versus total number of bins combined separately for each energy bin. The curves have been multiplied by factors as shown in the legend in order to space them out for clarity (the lowest energy bin is at the actual flux level observed). In both cases 95\% upper limits are indicated by a lack of error bars while detected fluxes (where the band TS has reached at least 10) are shown with gray error bars. }
    \label{fig:Light Curves}
\end{figure*}

The first radio knot in the jet of \pfs is located 1.3$''$ from the core location, which means that the inner jet is significantly affected by the wings of the PSF from the bright X-ray core. We conducted PSF simulations of the core in order to account for its contribution of flux to the inner jet. We used the toolset MARX, which provides ray tracing routines for the Chandra optics to simulate the PSF. We provided the aspect solution file from the observation and the spectrum extracted using \textit{specextract} from a 1.5'' (95\% ecf) radius centered on the core as inputs to MARX via the \textit{simulate\textunderscore psf} module in CIAO. The spectrum was modeled using an absorbed power-law model in SHERPA with the absorption column density set to a sum of an intrinsic column density and a Galactic column density in the direction of the quasar, the latter set fixed at $n_H$ = 7.13 $\times$ 10$^{20}$ cm$^{-2}$. The nuclear spectrum was well-fit by this model (reduced $\chi^2$ = 0.85) with a power law index $\Gamma$ = 1.75 $\pm$ 0.01. After performing 100 iterations of \textit{simulate\textunderscore psf}, a final model of the PSF was obtained by merging the outputs. The event file thus obtained was then binned to 0.2 times the native ACIS-S resolution in the 0.4-8~keV range to obtain a flux image at an effective energy of 1~keV. We then subtracted the flux from the inner knot of the simulated psf from the total flux of the jet resulting in an estimate of 14.8 $\pm$ 0.2~nJy at 1~keV. This is slightly less than the reported sum of knots in \cite{sambruna2004} of 19.6 $\pm$ 1.9~nJy. This is likely due to differences in measuring the total flux (we used a single contiguous region rather than 1$''$ radius circular regions on individual knots) and method of accounting for core contamination. We also fit the extracted jet spectrum as a power-law in SHERPA, yielding a spectral index $\alpha$ = 0.56 $\pm$ 0.11, which agrees with the \cite{sambruna2004} values for the individual knots within their (rather large) errors. Sub-pixel (1/5) binned \emph{Chandra} images of the jets are shown in Figure~1 with radio contours overlaid.

\subsection{\emph{Fermi/LAT}}

We utilized the progressive binning method to search for the minimum flux or upper limit in the five canonical \emph{Fermi}/LAT energy bands (0.1-0.3 GeV, 0.3-1 GeV, 1-3 GeV, 3-10 GeV and 10-100 GeV). The method used is identical to that described in \cite{meyer14} and \cite{meyer15} which we refer to for further details. Briefly, we used a 7 degree region of interest (ROI) to isolate photons observed by the \emph{Fermi}/LAT from the direction of the source over the time available at the time of analysis. For OJ 287 the mission elapsed time (MET) start and stop times are 239557417 to 577782027 and for \pfs they are 239557417 to 551014632. Using standard Fermi tools (version v11r5p3-fssc-20180124 for \pf, and conda-distributed version 1.0.2 for OJ~287) and the latest instrument response (P8R3\_V2) a light-curve was made for each source using bins of 1 week total Good Time Interval (GTI) time and an energy range of 100 MeV to 100 GeV. The light-curve was then reordered by test statistic (TS) value from lowest to highest value (where the TS is roughly significance squared). We then conducted a standard Fermi likelihood analysis on the source position for progressively combined bins -- first the lowest two, the lowest three, etc until all bins were analyzed together (the latter giving the average spectrum over the 10.5 years of Fermi observations). At each step in the recombined binning the flux (or upper limit) in each of the five \emph{Fermi} energy bands was calculated.  We then adopt the absolute minimum flux or upper limit in each band individually over the whole recombined binning to generate the minimum SED. In addition, for illustrative purposes we measured a `high state' composite spectrum by taking the ten highest bins (by TS value) in combination and producing the five band fluxes via maximum likelihood.

\section{Results}
The results of the \emph{Fermi}/LAT progressive binning analysis are shown in Figure~2. Here we plot either the 95\% upper limit (no error bars) or detected flux level (with error bars) for the source in each of the five energy bands versus the total number of bins combined (here the curves have been multiplied by regular factors as noted in the legend to space them out in the figure). As described above, the bins from the standard light-curve are first re-ordered from lowest to highest TS before being recombined sequentially as the two lowest, three lowest, etc for what we call the progressive binning analysis. Because of the low angular resolution of the \emph{Fermi}/LAT ($\gtrsim$~1$^\circ$) compared to the jets (tens of arcseconds), the fluxes and upper limits derived here apply to the core and large-scale jet combined.

\begin{figure*}[t]
    \centering
    \includegraphics[width=7in]{SEDs.eps}
    \caption{The SEDs for OJ~287 (left) and \pfs (right). The black data points (including X-rays) are the total flux in the large-scale jet, fit with a phenomenological model as in \cite{breiding2017}. The high-energy spectrum is the shifted IC/CMB curve as constrained by the synchrotron fit and the requirement to match the X-ray flux level. In the gamma-rays, three states of the source are shown as seen by the Fermi/LAT. The high state was measured by combining the highest ten (1-week) bins in the original light-curves. The `average' state is simply the total ten-year data set, while the `minimum' state is that derived from the progressive binning method described in the text. }
    \label{fig:SEDs}
\end{figure*}

The behavior observed in Figure~2 is slightly different for OJ~287 and \pf. For OJ~287, the source is initially not detected in any band. As the time-on-source increases, the flux limits generally decrease as expected (this is most dramatic in the highest energy band where the background is essentially zero) before the source is detected. For a source completely dominated by the variable core, the expected course after detection is to see steadily increasing fluxes since we have ordered the bins on significance (TS). However when dominated by a steady source, the expectation is that the detected flux level will remain steady while the error bars shrink. In the case of OJ~287, we do see signs of such `plateau' behavior consistent with a steady flux level in the highest energy band, with hints of a much smaller plateau in the middle three energy bands. This behavior is consistent with reaching a `floor' in the flux level due to the IC/CMB emission which is expected to be completely non-varying.

For \pf, the source is detected in every band except the last two even from the shortest combined bin, as shown at right in Figure~2. While the flux in each band is somewhat slow to rise, there is no clear sign of a plateau in any band. Thus either we are just barely able to detect the IC/CMB flux level before being overtaken by the brighter core, or the minimum-flux state of the core is coincidentally at the level expected for IC/CMB from the large scale jet under the assumption that the X-ray emission is entirely due to IC/CMB.

In Figure~3 we show the SED for each jet. The ALMA and \emph{Chandra} fluxes for the entire resolved jet outside the core, newly derived for this paper, are listed along with data from the literature in Table~1, where we also give the \emph{Fermi}/LAT (minimum) fluxes for the entire source. In Figure~3 the radio/sub-mm total jet fluxes are shown as black points with error bars, as are the \emph{Chandra} fluxes. The HST upper limits are also shown as black arrows. For the \emph{Fermi}/LAT observations we show three states of the source. In purple we show the `high state' SED made by compiling the 10 highest-TS bins from the original light-curve. In cyan we show the average SED as calculated from the entire time range of observations (10.5 years), and in dark yellow we give the minimum flux or upper limit for each of the \emph{Fermi}/LAT bands. Note that while the high and average state SEDs are generated from the same times on source, the low-state SED, by design, does not necessarily consist of fluxes measured from the same time-on-source. For OJ~287, the lowest flux/upper limit for each energy band occurred at combined bins 17, 4, 7, 10 and 16 from lowest to highest energy, respectively. For \pf, the values were taken from combined bins 7, 7, 1, 1, and 10.

In the IC/CMB scenario, the inverse Compton spectrum is essentially a copy of the synchrotron spectrum, shifted in frequency and luminosity according to the formulae in \cite{geo06} -- see also the discussion of the essential consistency between shifting the phenomenological curve and a more detailed physical model in \cite{meyer17}. As can be seen in Figure~3, the radio-optical synchrotron spectrum is reasonably well-constrained for both jets
and the \emph{Fermi}/LAT minimum flux values agree extremely well with the IC/CMB model predictions based on the radio to X-ray data for both jets.

\section{Discussion and Conclusions}

It has been nearly two decades since the first papers suggesting that the anomalously high X-ray emission from the jet of PKS~0637$-$752 could be due to the IC/CMB mechanism were published. In the intervening decades several dozen quasar jets have had their high X-ray fluxes explained in this way, though it was generally impossible to rule out the alternative scenario of a second synchrotron component or hadronic models. In more recent years the IC/CMB explanation for the X-ray emission in most of these cases has been ruled out via deep gamma-ray upper limits \citep{meyer14,meyer15,meyer17,breiding2017,breiding2018_thesis}; the interpretation being that most kpc-scale jets are not as fast and/or not as aligned as generally required in the IC/CMB model.

As originally explained in \cite{geo06}, the simplicity of the IC/CMB mechanism makes the predicted gamma-ray flux level inflexible given a well-sampled radio-optical synchrotron spectrum and a well-measured X-ray flux. The IC/CMB spectrum from the X-rays to gamma-rays has a shape set to match the radio-optical, and the normalization set by the X-rays. This normalization translates directly to a fixed value of B/$\delta$ where B is the magnetic field strength and $\delta$ the Doppler factor.
Regardless of whether IC/CMB can explain the observed X-ray emission, it is a mandatory process (ambient photons will inevitably be upscattered to higher energies) and will produce X-ray to gamma-ray emission at some level.

\begin{figure}[t]
    \centering
    \includegraphics[width=3.5in]{bapp_power_iccmb.eps}
    \caption{A comparison of OJ~287 and \pfs (cyan and red points) to 15 other X-ray jets for which IC/CMB was ruled out by \emph{Fermi}/LAT upper limits. On the x-axis is the jet kinetic power as scaled from low-frequency radio observations \citep[e.g.,][]{meyer11} and on the y-axis is the fastest recorded VLBI jet speed. Previous authors have noted an `envelope' in this plane with a forbidden zone at upper left \citep[e.g.][]{kharb2010}. This can be explained as a relation between $L_\mathrm{kin}$ and the intrinsic jet speed $\Gamma$, where sources at the upper edge of the envelope (which would run from lower left to upper right) are at the `critical angle' of $\theta\sim 1/\Gamma$.

    }
    \label{fig:Bapp_Power}
\end{figure}
In this letter, we argue that we have detected the IC/CMB emission from OJ~287 and \pfs based on the excellent agreement between the predicted level of IC/CMB based on the radio through X-ray SED and the minimum flux level in the GeV band. The case is particularly strong for OJ~287 where we observe a plateau signature in the recombined light-curve which is consistent with a steady floor to the GeV flux.  The case for \pfs is less strong due to the lack of this signature -- it is possible that we have simply measured the minimum flux level of the core from the last ten years of \emph{Fermi/LAT} observations which coincidentally matches the level and spectrum expected from the jet under IC/CMB. Continued long-term monitoring by the \emph{Fermi}/LAT will clarify this issue. If the minimum-flux state currently measured is due to the core, then it is likely that in the next several years the core will reach even lower flux states as part of its overall variability. In that case we would see the measured GeV minimum-flux begin to dip down below the prediction shown in Figure~3, and we would have to rule out IC/CMB as the source of the X-ray emission in this source. On the other hand, if the minimum-flux state really is IC/CMB, then future observations of the source when the core is (inevitably) in a low state \emph{below} the steady emission of the large-scale jet will produce a plateau in the progressive binning curve. At present we favor the IC/CMB interpretation of the GeV minimum state in \pfs simply because it would be unlikely for the core to match the expected level and spectral shape by chance. It also seems likely that the flux measured in the 10-100 GeV band for \pf, which is somewhat above the IC/CMB prediction, is contaminated by the core (the minimum value in that band comes from the most time-on-source at 10 combined bins compared to only 1 bin in the previous two bands).

\begin{deluxetable*}{llllll}[th]
\tabletypesize{\small}
\tablecaption{\label{apptab1}Flux Measurements}
\centering
\tablehead{ Source & $\nu$ (Hz) & $\nu F_{\nu}$  & Source & $\nu$ (Hz) & $\nu F_{\nu}$  \\
 & (Hz) & (erg s$^{-1}$ cm$^{-2}$) &  & (Hz) & (erg s$^{-1}$ cm$^{-2}$) }
\startdata
OJ~287  & 1.4 $\times$ 10$^{9}$   &  1.52 $\times$ 10$^{-16}$ (a)         & \pfs &  1.5 $\times$ 10$^{9}$  &  3.15 $\times$ 10$^{-15}$ \\
        & 4.8 $\times$ 10$^{9}$   &  1.98 $\times$ 10$^{-16}$ (a)        &            &  4.9 $\times$ 10$^{9}$  &  4.53 $\times$ 10$^{-15}$ \\
        & 1.5 $\times$ 10$^{10}$  &  2.14 $\times$ 10$^{-16}$ (a)         &            &  1.45 $\times$ 10$^{11}$  &  1.21 $\times$ 10$^{-14}$ \\
        & 5.2 $\times$ 10$^{14}$  &  $<$1.04 $\times$ 10$^{-16}$ (a)      &               &2.33 $\times$ 10$^{11}$  &  1.07 $\times$ 10$^{-14}$  \\
        & 2.4 $\times$ 10$^{17}$  &  2.49 $\pm$ 0.07 $\times$ 10$^{-14}$  &            &  3.43 $\times$ 10$^{11}$  &  1.00 $\times$ 10$^{-14}$  \\
        & 4.19 $\times$ 10$^{22}$  &  2.40 $\pm$ 0.78 $\times$ 10$^{-12}$&            &  5.1 $\times$ 10$^{14}$  &  $<$4.08$\times$ 10$^{-16}$ (b)  \\
        & 1.32 $\times$ 10$^{23}$  &  2.98 $\pm$ 1.09 $\times$ 10$^{-12}$ &            & 2.4 $\times$ 10$^{17}$  &  3.72 $\pm$ 0.05 $\times$ 10$^{-14}$   \\
        & 4.19 $\times$ 10$^{23}$  &  1.67 $\pm$ 0.68 $\times$ 10$^{-12}$&            & 4.19 $\times$ 10$^{22}$  &  2.36 $\pm$ 0.25 $\times$ 10$^{-11}$  \\
        & 1.32 $\times$ 10$^{24}$  &  1.38 $\pm$ 0.70 $\times$ 10$^{-12}$&            & 1.32 $\times$ 10$^{23}$  &  2.09 $\pm$ 0.19 $\times$ 10$^{-12}$  \\
        & 7.65 $\times$ 10$^{24}$  &  $<$6.52 $\times$ 10$^{-13}$      &            & 4.19 $\times$ 10$^{23}$  &  9.35 $\pm$ 4.31 $\times$ 10$^{-12}$ \\
        &                      &                               &         & 1.32 $\times$ 10$^{24}$  &  $<$4.69$\times$ 10$^{-12}$ \\
        &                      &                               &         & 7.65 $\times$ 10$^{24}$  &  2.12 $\pm$ 1.37 $\times$ 10$^{-12}$ \\
\enddata
\tablenotetext{a}{\cite{marscher2011}}
\tablenotetext{b}{\cite{sambruna2004}, otherwise this paper}
\end{deluxetable*}

The detection of IC/CMB implies a value for B/$\delta$ for each source. We have calculated equipartition values of B$\delta$ of 2.9 $\times$ 10$^{-5}$ G and 6.1 $\times$ 10$^{-5}$ G for OJ~287 and \pf, respectively, based on the 1.4 and 5 GHz radio observations and an assumed minimum electron Lorentz factor $\gamma_\mathrm{min}$ of 10. Using these values, the required Doppler factors $\delta$ are 22.5 and 19 to match the gamma-ray minimum level.

Given the results of our larger study of X-ray jets which are generally \emph{not} emitting X-rays dominated by IC/CMB, one must ask what makes these sources so different. While IC/CMB should increase significantly with redshift due to the $(1+z)^4$ enhancement of the CMB, these sources are not high-redshift at $z\sim0.3$. However, it is notable that each is highly superluminal on parsec scales, especially relative to their jet powers. OJ~287 has a maximum observed jet speed from Very Long Baseline Interferometry (VLBI) measurements of 20.1$c$ \citep{homan2001}, while \pfs has a maximum of 47$c$ \citep{jorstad2005}. Such high values immediately imply very small maximum orientation angles of 5.7$^\circ$ and 2.4$^\circ$ respectively. Further, when compared with other {Fermi}-detected X-ray jets, these speeds make them clear outliers. In Figure~4 we plot the apparent speed versus kinetic jet power for 15 jets where \emph{Fermi}/LAT has \emph{ruled out} IC/CMB as the source of the X-ray emission (data taken from \citealt{breiding2018_thesis} and forthcoming Breiding et al., 2019) as black triangles. The two subjects of this paper are noted as a cyan triangle and red circle, labeled.

We argue that these sources are rare cases of orientation at the critical angle near 1/$\Gamma$ where $\beta_\mathrm{app}$ is maximized. In such cases the jet is just misaligned enough so that the large-scale jet is visible as an arcsecond-scale jet in high-resolution imaging, while being aligned enough that the (inevitable) IC/CMB emission is boosted significantly and dominates over the (presumed) synchrotron X-ray emission. The sensitivity to angle is considerable. As an illustration, let us assume that the jets have Lorentz factors of 22 and 50 and are oriented at the critical angle of 1/$\Gamma$, or 2.6$^\circ$ and 1.1$^\circ$ for OJ~287 and \pf, respectively. The beaming pattern for IC/CMB emission scales as $\delta^{4+2\alpha}$ (here we let $\alpha$=0.5), so at the assumed $\Gamma$ values the orientation angles of the two sources would need to increase to only 3.8$^\circ$ and 1.6$^\circ$, respectively for the IC/CMB X-ray emission to drop to 1/10th of the observed value. Given that the majority of similar (presumably more misaligned) sources in our larger sample appear to be dominated by synchrotron X-ray emission, this would likely dominate over the IC/CMB emission at most orientations.

There is another factor which likely makes these jets outliers in addition to the orientation angle. As noted previously, population-based evidence as well as individual limits on $\delta$ from both proper motions \citep[in 3C~273;][]{meyer16} and deep \emph{Fermi}/LAT limits on the IC/CMB emission imply most large-scale jets are only mildly relativistic. Here we require high values of the Lorentz factor on extremely large scales -- assuming the maximum angle, the jets in OJ~287 and \pfs deproject to lengths of at least 600 and 800 kpc.  It is possible that only a few jets are able to accelerate flows and maintain high $\Gamma$ values at such distances. Such lengths also imply that these jets are not young. Interestingly, recent work on realistic GRMHD models of jets have trouble producing values of $\Gamma$ as high as are implied in the population (i.e., $\Gamma >$ a few), except where empty `channels' have been previously excavated, presumably by earlier jet activity (e.g., \citealt{bromberg2016}; see also the discussion in \citealt{marscher2011}).

 In many cases the IC/CMB model requires super-Eddington jet power, but we find that is not required here, as was also found previously by \cite{marscher2011} for OJ~287. The minimum required power under the IC/CMB model is $1.8\times 10^{45}$ and $1.2\times 10^{45}$~erg~s$^{-1}$ for OJ~287 and \pfs respectively.

 Estimates of the black hole masses for OJ~287 and \pfs are moderately but not extremely large, at $10^{8.79}$ and $10^{8.62}$ $M_\odot$ \citep[][scaled from H$\beta$ width]{wang2004} yielding an Eddington luminosity of 5$-$8 $\times$ 10$^{46}$~erg~s$^{-1}$, which leaves a comfortable margin for the power requirements of the IC/CMB model even if one relaxes significantly away from the minimum. Interestingly, the estimated kinetic power of these jets, scaled from the low-frequency radio luminosity (\citealt{meyer11}, also Keenan et al., in prep.) is 7.4 $\times$ 10$^{43}$~erg~s$^{-1}$ and 1.1 $\times$ 10$^{45}$~erg~s$^{-1}$ for OJ~287 and \pf, respectively.  While the latter is a good match to the IC/CMB power requirements, for OJ~287 the discrepancy is considerable. However it has been shown that environment likely plays an important role in the large scatter of jet power/radio luminosity scalings \citep{hardcastle2013} and it is not clear that the low-frequency radio estimates of power are reliable for individual sources.

Ultimately, it seems likely based on the full body of recent results which rule out the IC/CMB model for most X-ray jets, that OJ~287 and \pfs will prove to be outliers, with a particularly favorable alignment and unusually high jet speed at large distances. Indeed, it seems sources with Lorentz factors of 10-20 on nearly Mpc scales must be very rare, or else a similar case would have been confirmed much earlier, had the angle to the line of sight been even more favorable: halving the angle for either of these jets would produce a shorter, but still visible and extremely bright X-ray jet and even higher steady gamma-ray flux. Given the $(1+z)^4$ enhancement of the CMB and larger volume probed with redshift, it is likely that high-redshift counterparts to these unusual jets will eventually be found -- a promising candidate is the recently detected X-ray jet with very weak radio emission at $z$=2.5 \citep{sim2016}.

\acknowledgments
\noindent
E.T.M acknowledges NASA Fermi grants NNX15AU78G and 80NSSC18K1733.~E.T.M. and M.G. acknowledge NASA ADP grant NNX15AE55G and NSF grant 1714380.

\noindent
This paper makes use of the following ALMA data:
\begin{itemize}
  \setlength{\parskip}{0pt}
  \setlength{\itemsep}{0pt plus 1pt}
    \item ADS/JAO.ALMA\#2016.1.00406.S
    \item ADS/JAO.ALMA\#2016.1.00116.S
\end{itemize}
\vspace{-\topsep}
\noindent
ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.

\vspace{5mm}
\facilities{VLA, ALMA, HST, Chandra, Fermi}

redpajama_set_name: RedPajamaArXiv


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Information about the Midwest Conference on Technology, Employment and Community held in Chicago, March 2-4, 1995.
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text:
E-bikes & Emerging Technologies
Trail Capacity
Trail Inventory
Tread Surface Erosion Control
Youth Corps
Connecticut: Russ Waldie
Russ Waldie is a dedicated and reliable volunteer section maintainer on the Appalachian Trail in Connecticut, and has been for more than a decade.
Delaware: Meinrad Leckie
In 2011-2012, Meinrad Leckie volunteered over 300 hours on a variety of trail projects across northern New Castle County Delaware.
Hawaii: Fred Bannan
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Illinois: Eileen Weyhrich
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Kentucky: Mike Bossert
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Louisiana: Freddie Paul
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Related images in Management and Maintenance
Sign direction trail users down dead-end street to continuation of trail in La Conner, Washington
Both motorized and nonmotorized trail activities are allowed on this Ashland, Wisconsin trail. Trail is used for both winter and summer activities.
Related businesses in Management and Maintenance
Eco-Counter, Inc.
R.J. Thomas Mfg. Company Inc. / Pilot Rock


Will Obama Destroy Any Hope of U.S. Energy Independence?
The U.S. consumes nearly three times the amount of oil that it produces domestically on a daily basis. How can this statistic get any worse, you might ask?
Imagine in 2010 the Obama administration persuades Congress to pass a budget that results in a reduction of domestic oil production by 10% - 20%, making the supply/demand imbalance even more lopsided. Foreign oil companies will gain a distinct advantage over American domestic operators as an unintended consequence of these proposals.
Sound farfetched? It's closer to reality than you may think… If it comes to pass, it will likely be the biggest structural change in the U.S. domestic oil and gas industry in decades and have far-reaching implications for investors and for the entire country.
In early 2009, the Obama administration proposed to eliminate significant tax incentives for the oil and gas industry. These tax benefits were put in place decades ago to incentivize oil and gas producers to develop domestic sources of energy, while recognizing that oil and gas exploration entailed special risks. Two of the proposed repeals with the most potential impact relate to what the industry refers to as "percentage depletion" as well as "intangible drilling costs" (IDC).
The first proposal involves eliminating the deduction for percentage depletion. Currently, the tax code allows small oil and gas producers to choose between two different tax deductions, percentage depletion or cost depletion (Big Oil's ability to use percentage depletion was severely limited years ago).
Percentage depletion allows a tax deduction of 15% of the annual gross revenue of a well, continuing as long as the well produces and even after 100% of the costs have been recovered. On the other hand, cost depletion is calculated as the amount of oil or gas produced annually as a percentage of the total reserves of the reservoir. This deduction ceases when 100% of costs have been recovered (after which the producer may switch to percentage depletion).
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And cost depletion is pretty much out of the question for most small stakeholders, as it's extremely difficult for them to calculate. Small stakeholders in wells often aren't entitled to the proprietary reservoir data developed by the operator of the well, which is necessary to calculate cost depletion. While the operators do disclose reservoir data in their annual reports, they rarely contain enough detail for a small stakeholder to locate information relating to a small field or well in which the stakeholder has an interest. Oil and gas stakeholders – such as individual royalty owners, royalty trust investors, and landowners, who all benefit from leasing land to oil and gas explorers – will immediately see the value of their investment decrease while simultaneously paying more in taxes every year.
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text:
const helpers = require('../utils/helpers');
const mcpi = require('../../src/');

describe('World', () => {
  it('setProperty', (done) => {
    const mc = helpers.mc();

    mc.world.setProperty(mcpi.WorldSettings.WorldImmutable, true)
      .then(() => mc.world.setProperty(mcpi.WorldSettings.WorldImmutable, false))
      .then(() => mc.close())
      .then(done)
      .catch(err => {
        mc.close();
        done.fail(err);
      });
  });
});

redpajama_set_name: RedPajamaGithub


The game is the brainchild of Scots corporate troubleshooter Tim Dew, Stuart Laing and Mike Perrin.
An Edinburgh-based start-up that aims to revolutionise training in critical decision-making is set to launch this summer after a £500,000 investment.
The new company Games Without Frontiers is unveiling an artificial intelligence-powered training and development "game" which lead its players through a series of simulations that mirror the real-life challenges of managing a growing business.
The brainchild of Scots corporate troubleshooter Tim Dew, business simulation expert Stuart Laing and former Skyscanner technical manager Mike Perrin, GWF is rolling out its first product Rocket, touted as the first ever AI-enabled business training game.
By playing the game, participants enhance their skills and capacity, learning necessary hard lessons without negative effects on their "real" company's bottom line.
Edinburgh-based GWF, which currently employs seven people has already piloted the Rocket game, developed with the founders own cash investment. It presents realistic simulations of developmental stages in the life of a family-owned manufacturing company in an "accelerated time environment". The company has launched a word-of-mouth marketing campaign based on trial "roadshows" for invited contacts in Edinburgh and Glasgow and has scheduled a series of further invitation-only sessions in Dundee, Aberdeen, Inverness and London.
The launch product Rocket simulates a provincial confectionery manufacturer scaling up to supply nationwide wholesale and retail operations. Further company scenario games are currently in development, including ones aimed at the entrepreneurial incubator market, at the large corporate environment and one for the finance industry.
"As a company we believe that, as SMEs account for around 50% of the GDP of the UK, improving their performance by even the smallest amount could have a massive potential impact on the UK economy".
Gilchrist describes how Dew approached colleagues with the concept for the game based on the "experiential learning" teaching of the US business theorist David Kolb.
"Through Q1 of 2017, they moulded a vast wealth of business challenges, experience and learnings into a four-round game. It was initially paper based, before they sought out Mike Perrin who they knew had the IT and coding skills to craft components required to develop a game that delivers understanding of how to run a business to every participant.
Rocket, which will be marketed and charged as a full-day experience at around £5000 a day for a company team of 5 to 12 is played in a room subdivided into "pods".  Teams of players are assigned roles, such as marketing, sales, accounts, production or managing director. They are presented with a series of tasks that rely close co-ordination with their "colleagues" in other parts of the "company".
After further trials and tweaks, the product goes out to market mid-September. Backers are confident that word of mouth will generate initial sales, and are working on incentivisation structures for players who recommend it to contacts, while understanding that participants are only likely to recommend Rocket unless it fulfills the claims that its creators are making. No-one wants to recommend business training unless it "works" - or not if they expect to please their contacts and keep their friends.