Miss Diana Krall gave a bravura performance in the Shed on the opening weekend of 75th season of concerts at Tanglewood. The show featured a crackerjack combo Anthony Wilson (guitar), Robert Hurst (bass), and Karriem Riggins (drums) in support of an almost wierdly diverse setlist that visited many provinces of the jazz empire. While it wasn't the sort of program Miss Mary Aspinwall Tappan had in mind in 1936, when she laid the family cottage (and 210 sylvan acres) on Maestro Koussevitsky (and the BSO), it was the sort we locals have become accustomed to while the BSO has become an increasingly important element of life in the Berkshires*.
Since her first Tanglewood apearance years ago, on a bill as Tony Bennett's guest, when "show-stealing siren" could've been an apt description, Miss Krall has become a full-fledged star with a commanding stage presence and an easy rapport with the audience. That was especially evident during the solo portion of her two hour set when she led into several numbers with references to her parents; and talked about her 5 year old twins. (She made a surprise appearance just before their birth during husband Elvis Costello's performance on Marian McPartland's Piano Jazz during the 2007 Tanglewood jazz Festivl).
Miss Krall's artistry is a melding of her voice and the piano; combined with her personality and musical sensibility, tonight's two hour concert thouroughly satisfied. Her band was equally brilliant, bass and drums blending in primarily supportive roles, but bassist Robert Hurst had some prominence, including one passage where he brought a song home with descending notes until perfect silence was made to reverberate.
Guitarist Anthony Wilson alternated between solo and support all night, as well as being Miss Krall's go-to guy in deciding the setlist. He played several leads and riffs that excited the audience, and altogether produced the perfect complimentary sound to Miss Krall's.
Her setlist drew from the work of Fats Waller, Nat King Cole, Peggy Lee, Sergio Mendes, Tom Waits, and Bob Dylan and included a stunning rendition of John Lennon's Come Together. Since Quiet nights was released in 2009, Krall has performed on four continents, produced Barbra Streisand's Love Is the Answer, contributed Simple Twist of Fate to the charity album Chimes of Freedom: The Songs of Bob Dylan Honoring 50 Years of Amnesty International and performed on Paul McCartney's new album, Kisses On The Bottom.
Opening the show were the Canadien duo Denzell Seymore and Devon Thompson; really tasty music, but just too much patter for an un-familiar opening act.
*We overheard a conversation – someone was bemoaning the Berkshires remoteness from the ocean or the great lakes – her interlocutor said true enough, but can't you imagine Tanglewood as a sort of ocean where wave after wave of great music washes ashore?


text:
Q: Printing an image for each object in an array with React Native I'm pretty new to React Native and got stuck on a personal project trying to utilize Instagram's API. I'm currently using a forEach to try to return an Image for every object in an array and it doesn't seem like I can get the Image to show up. When I do a console.log(images.images.thumbnail.url) within the mediaPrinter function, I do see that all the urls are being logged.
Here's the API call:
export default function ApiCall() {
  return fetch(url)
      .then((response) => {
        return response.json()
      })
      .then((json) => {
        return json.data
      })
      .catch((error) => {
        console.log(error)
      })
}

And the rest of the relevant code:
mediaPage() {
  return <ScrollView style={styles.scrollBody}>
      <Text style={styles.welcome}>
          Browse Through Our Moments
      </Text>
      <View style={styles.imageRow}>
        {this.mediaHandler()}
      </View>
    </ScrollView>
}

mediaHandler() {
  ApiCall()
    .then((data) => {
      this.mediaPrinter(data)
    })
    .catch((error) => {
      console.log(error)
    })
}

mediaPrinter(array) {
  array.forEach(function(images) {
    return <Image
      source={{uri: images.images.thumbnail.url}}
      style={{width: 138, height: 138}} />
  })
}

I was also wondering if there was a way to resize the images responsively using React Native's currently provided resources.

A: This should do the tirck:

class renderImages extends Component {
  constructor () {
    super()
    this.state = {
      images: []
    }
  }

  componentDidMount () {
    this.mediaHandler()
  }

  mediaPage() {
  return <ScrollView style={styles.scrollBody}>
      <Text style={styles.welcome}>
          Browse Through Our Moments
      </Text>
      <View style={styles.imageRow}>
        {this.mediaPrinter(this.state.images)}
      </View>
    </ScrollView>
}

mediaHandler() {
  ApiCall()
    .then((data) => {
    this.setState({images: data})
      //this.mediaPrinter(data)
    })
    .catch((error) => {
      console.log(error)
    })
}

mediaPrinter(array) {
  return array.map(function(images, index) {
    // don't put your key as index, choose other unique values as your key.
    return <Image
      key={index}
      source={{uri: images.images.thumbnail.url}}
      style={{width: 138, height: 138}} />
  })
}

}

The function you called inside the <View style={styles.imageRow}></View> should return jsx to be rendered. As you can see, in your approach, you are returning nothing.
In the solution above, I have set the state when medialHandler gets data from instagram, which triggers the re-render and the mediaPrinter function is called again with the array of instagram photos data, hence it gets rendered.

A: mediaHandler() returns promise. React don't know anything about promises. So react can't render your image list.
You should not mix any non-ui logic and rendering inside component. It is bad practice. React ui component should be as stupid as possible. Component should only render ui based on data passed throw props (image list in your case) and trigger some events (image click for example). Calling API is work for another part of your code.
There are many possibilities how to write your code. One of them is concept of "clever" (container) and "stupid" (presentation) components.
In your case presentation component will be:
class ImageList extends React.Component {
  render() {
    return <ScrollView style={styles.scrollBody}>
             <Text style={styles.welcome}>
               Browse Through Our Moments
             </Text>
             <View style={styles.imageRow}>
               {this.renderImages(this.props.images)}
             </View>
           </ScrollView>;
  }

  renderImages(images) {
    return images.forEach(function(image) {
      return <Image
        source={{uri: image.url}}
        style={{width: 138, height: 138}} />
    })
  }
}

And container component:
class ImageListContainer extends React.Component {
  constructor() {
    super();
    this.state = { images: [] }
  }

  componentDidMount() {
    ApiCall()
      .then((data) => {
         ...
         this.setState({images: images})
      })
  }

  render() {
    return <ImageList images={this.state.images} />;
  }
}

More info you can find here https://medium.com/@learnreact/container-components-c0e67432e005#.r8c3p0540 and here https://medium.com/@dan_abramov/smart-and-dumb-components-7ca2f9a7c7d0#.65028sqwh
Another option is using redux, flux, rx or whatever you want. React provides only presentation layer.

redpajama_set_name: RedPajamaStackExchange


text:
The UAE ticks all the right boxes for start-ups
Our nation is a big hub of technology and innovation, as Dubai is the centre of gravity in that space
Raja Al Mazrouei, Executive Vice-President of Fin Tech Hive at DIFC. (Photo by Shihab)
By Raja Al Mazrouei
Published: Fri 3 Dec 2021, 2:12 PM
Dubai has emerged as a flourishing fintech hub for the Middle East and the North Africa (Mena) region because of the vision and able leadership of His Highness Sheikh Mohammed bin Rashid Al Maktoum, Vice-President and Prime Minister of the UAE and Ruler of Dubai.
The emirate has been ticking all the right boxes since the start of the new millennium to attract startups. Data shows that the digital economy contributes about 4.3 per cent to the UAE's gross domestic product (GDP), or around Dh100 billion. Dubai is the hub for the bulk of the 1,400 startups, 90 investment funds in the digital sector and 12 business incubators, whose cumulative valuation is estimated to be around Dh90 billion.
The outlook is rosy and will grow further because of the UAE's bid to embrace digital transformation, especially in the FinTech sector, and the country is on a par with New York, Berlin, London and Singapore.
For instance, Dubai had introduced a raft of reforms and initiatives last November, including changes to personal and family laws in the country and a retirement visa scheme. The move was aimed to make our country more expat-friendly.
Our nation is a "big hub of technology and innovation" as Dubai is the centre of gravity in that space.
The DIFC FinTech Hive is one of the driving forces of innovation for it is the first and largest financial technology accelerator in the Middle East, Africa and South Asia (MEASA) region, as it is located in the heart of DIFC, and as part of the DIFC Innovation Hub that is home to over 350 innovation companies. T
he FinTech Hive's highly competitive flagship FinTech accelerator program is run in collaboration with the region's leading financial institutions such as ADIB, ENBD, Standard Chartered Bank, Visa, Zurich and more who work with selected start-ups each year in developing their solutions to collaborate in integrating and offering new products and services.
Over the past few years, the accelerator has successfully driven the growth of FinTech, InsurTech, RegTech and Islamic FinTech startups looking to tap into the MEASA market and capitalise on unlimited opportunities in the region by connecting them with top tier organizations in each vertical.
As it stands, the FinTech Hive has accelerated over 120 startups through its programmes, and FinTech firms based in DIFC have now raised more than Dh1.1 billion ($298.8 million). Furthermore, the FinTech Hive's efforts have expanded to include the AccelerateHer programme, our female talent and career mentorship program that we launched to support and empower women in financial services and help them play a more active role in the development of the region's financial services landscape.
The programme to date has conducted over 60 dedicated workshops with 48 mentorship pairings and we plan on increasing the size of our cohort each year to ensure women have the platform to develop and progress in their careers.
Our ambitions at the FinTech Hive grow each year as we strengthen our ecosystem partnerships across various industries and grow our global hub network around the world to harness innovation and creativity and continue disrupting the financial services industry.
Our nation is a big hub of technology and innovation, as Dubai is the centre of gravity in that space.
(The author is the Executive Vice-President of FinTech Hive at DIFC)
More news from Year of the 50th
Cyber safety training must be compulsory to combat attacks
The biggest, most damaging and largely widespread threat faced by many organisations, even individuals, are phishing attacks
Year of the 50th1 month ago
Tech innovations in the UAE will only continue to rise
UAE will become faster at adapting to trends and more importantly, setting them
Look: Indian FM attends 50th UAE National Day reception
A video depicting the country's growth in the last 50 years was screened at the event.
Films in the future will showcase Emirati stories for evolving global audience
A tremendous number of untold stories from Dubai's olden days need to be shared with the world; they need to be brought to the big screen
US congratulates the UAE on Golden Jubilee
US Secretary of State, Antony Blinken, wishes the country peace and prosperity
Look: UAE resident's portrait of Sheikh Zayed was created with 35,000 scarf pins
Anil Kumbanad took 98 hours across a week to complete the work
UAE National Day offer: Get free 50GB mobile data for next 6 months
More special deals have been announced to celebrate the Golden Jubilee
Watch: Rahat Fateh Ali Khan sings Watan, the Urdu version of UAE National Anthem
This is the first time Ishy Biladi has been translated into another language from Arabic

redpajama_set_name: RedPajamaCommonCrawl


Get fresh with your accessories by mixing and matching your menswear staples with this effortlessly handsome striped tie in luxurious shades of teal blues and coffee browns. The charming color combination is remarkably versatile and looks sharp paired with a broad range of menswear colors and textures.
One of our favorite looks this season is seeing this dynamite tie paired with a white cotton button down, a chic taupe blazer and broken in chinos. This incredible necktie is a signature design from the Cavallieri Luxury Edition Collection. Made from 100% silk.
"Ordered for a wedding. Great description and perfect color match!"
"I was looking for a tie with chocolate brown and teal for my husband to wear with his brown suit and to co-ordinate with my teal gown for a formal wedding we are attending. This one turned out to be perfect."
"This Teal and brown stripe tie is stunning with a brown suit. Many compliments when he wore it."


If you like fast, furious fishing action then now's the time to take a trip to Lake Powell.
Striped bass have started to feed on the surface, where they are relatively easy to find and catch. Schools of stripers attack schools of tiny shad. Shad often leap out of the water in a frenzied attempt to escape, with stripers in hot pursuit. The intense action makes the water appear to "boil" in productive spots. Retrieve a shad-imitating lure through a boil and stripers will pound it aggressively.
You've got to hunt down the boils but when you find one action can be incredibly fast. It's my favorite fishing experience. Mostly small fish are boiling now but larger fish will soon join the party. Action will get better and better during the next few weeks, peaking in late August or early September.
Study this website to learn to catch the fish. It is updated frequently and offers current, accurate information.
Small stripers were boiling up and down from the mouth of White Canyon on 7-22, mid-afternoon. We chased them for an hour and caught 10-13 inchers until our arms were tired.
We camped in a cove across and just down-lake from White. An algae bloom brought a bazillion shad into the cove. There was a large boil right in our cove just before sunset. After the stripers left we kept casting and caught several nice smallmouth (the biggest is shown in the attached photo).
A short boil occurred in our cove the next morning.
Saw a coyote twice while camped in that cove.
We launched at Hite, using the road base where the marina store was located. It was easy pushing my little fishing boat out into the channel, which was only four feet deep. Had to squeeze between brush, but that wasn't hard. Water level was approximately 3608.55. I took a look at the main Hite ramp and decided not to attempt to launch there. It was obvious people trying were getting stuck in the mud.
On 7-21 we were down at Slickrock Canyon and found smallmouth bass boiling near the brush in the back of the canyon. Caught a bunch of smallies, 7-10 inchers, and one tiny striper.
A rattlesnake tried to climb under our tent to get out of the rain while we camped near Slickrock. It buzzed when it felt us moving around. I peeked out the door it was coiled right against our tent. It was probably 3.5 feet long. It buzzed for about 10 minutes and then slithered away.
A bill passed by US Congress Monday designates two Utah highways (and associated small communities) as "national heritage areas." The bill now goes to President Bush for his signature, which is expected to come quickly without any controversy.
A portion of US Hwy 89, long known as Utah's Heritage Highway, was designated the Mormon Pioneer National Heritage Area. The section stretches between Fairview, Sanpete County, and the Arizona border.
The bill also created the Great Basin National Heritage Route, between Delta, Juab County, and Ely, Nev.
This Deseret Morning News article provides more detail.
After months of preparation, a team from Honda reached a measured mile speed of 400kph on the Bonneville Salt Flats last week, setting three new world land speed records and also setting a new top speed for a Formula One car.
The first pioneers arrived in the Salt Lake Valley on July 24, 1847. Ever since then, July 24 has been set aside as a state holiday, with events galore celebrating our pioneer heritage.
Friday, 7 pm: Pioneer Day Concert at the Conference Center in downtown Salt Lake City featuring the Mormon Tabernacle Choir and Orchestra at Temple Square.
Saturday 10 am: Youth Parade beginning at 600 E. 500 South, Salt Lake City; followed by Youth Festival with games, crafts, rides and food at Washington Square, 450 S. State, until 1 p.m.
Saturday, 6-11 pm: Celebration of Utah's Cultures at the Gallivan Center, 239 S. Main St., Salt Lake City.
Saturday, 7 pm: World Championship Rodeo at the Delta Center; tickets are $12.50 to $39.50, at the box office or 801-325-SEAT.
Monday, 7 am: Sunrise Service at the Assembly Hall on Temple Square, 7 a.m.
Monday, 9 am: Days of '47 Parade, starting at South Temple and Main Street.
Monday, 11 am to 6 pm: Pioneer Festival at This Is the Place Heritage Park, 2601 E. Sunnyside Ave.
Monday, 7 pm: World Championship Rodeo at the Delta Center, 7 p.m.
On Monday there will also be a Native American Celebration at Liberty Park, 500 E. 900 South, Salt Lake City, 7 a.m. to dusk. There will be food booths, entertainment, arts and craft booths; the 12th Annual Intertribal Competition Powwow begins at noon, with an intermission at 4 p.m.; second session begins at 5 p.m. The fireworks grand finale is at 10:10 p.m. This event is free.
The Tribune forgot to mention the KJZZ-TV/Deseret Morning News Marathon/10k. It will be held Monday morning, beginning at 5:30 am. The marathon ends at Liberty Park.
Here's an official list of events.
Utah Governor Jon Huntsman and the Nature Conservancy yesterday launched what they call the largest land preservation and restoration campaign in state history.
The "Living Lands and Waters initiative" will raise $43 million in public and private funds for conservation projects to save Utah's most at-risk lands and waters, according to a Nature Conservancy press release.
To date, the Conservancy has raised $24.9 million in public and private funds, leaving $18.1 million to be raised by the target date of July, 2009.
To coincide with the launch of the campaign, the Conservancy announced the purchase of a conservation easement on the 6,700-acre Selman Ranch near Logan. Nestled in the Little Bear drainage, this ranch harbors breeding ground for the Columbian sharp-tailed grouse—a bird that has already lost more than 96 percent of its historic habitat in Utah and is in danger of being federally listed as an endangered species.
Virgin River Headwaters: a conservation collaboration among 17 ranchers on 11,000 acres near Zion National Park, supporting critical habitat and a key watershed.
Boulder Creek Canyon Ranch: the protection of prime ranchland in the heart of Boulder, creating a wildlife corridor between natural protected areas.
Great Salt Lake: the Wings & Water Wetlands Education Program offers 4th grade students and teachers a new way to use the Great Salt Lake as an unforgettable outdoor classroom.
White Dome: a new 800-acre preserve in Washington County will create a community resource and save some of the world's last remaining populations of endangered wildflowers.
A flash flood watch has been issued for southern Utah this afternoon and evening, for Washington, Iron, Beaver, Garfield and Kane counties. Here are watch details.
Numerous thunderstorms are expected and rain may be heavy in spots. The heavy rain could cause rapid water rises and flows in creeks and dry washes across the region. People traveling and recreating in these areas should use caution. Do not hike in wash bottoms or narrow canyons and don't camp in wash bottoms.
Thunderstorm and flash flood danger may develop again tomorrow afternoon (7-19).
Wildfires recently closed I-15 near Cove Fort in central Utah and near Pintura in SW Utah. Those two fires are not contained but are no longer burning near the Interstate and so traffic is flowing normally at this time. However, both fires have the potential to threaten the Interstate again. If that happens the freeway may be closed again until the danger is past.
The Kolob Canyons district of Zion National Park is closed because of the fire.
Thunderstorms may help or hamper the effort to control the wildfires. Rain can beat back the flames, but wind may cause the fire to spread rapidly and erratically. Lightning associated with thunderstorms may ignite new fires.
This website has the latest info on Utah wildfires.
At team from Honda will be on the legendary Bonneville Salt Flats this week attempting to set an outright land speed record for a Formula One car.
"Next week sees the climax of a long two-year project for the Honda Racing F1 team. We hope that the result on the Salt Flats will reflect the hard work and dedication that has been put into this project by all the team both in the UK and Japan".
The snow is completely gone, the trails have dried out and now mountain bikers have taken over the mountains surrounding Park City, Utah.
The popular ski resort town is a hub for summer adventure, with hundreds of miles of biking and hiking trails stretching in all directions. Nearby Jordanelle and Deer Creek reservoirs offer excellent opportunity for boating and water sports and the fabled Provo River is a top destination for fly fishermen looking for trophy trout.
Deer Valley is becoming a major destination for mountain bikers. The resort offers lift-served access to over 50 miles of excellent, panoramic trails. Bikers are whisked up the mountain on the Silver Lake Express chairlift from Snow Park Lodge, or this summer they can also ride the Wasatch Express chairlift, located mid-mountain.
Silver Lake Express operates daily from 10 am to 5:30 pm (with last chair downloading at 5 pm). Wasatch Express operates daily from 10 am to 5 pm (with last chair downloading at 4:30 pm). An all-day bike pass is $22; a single-ride bike pass is $14; a season pass is $250 and an interchangeable hospitality pass is $500.
Deer Valley's Mountain Bike Rental Shop and Mountain Bike School are open daily and offer scheduled clinics and tours for all abilities. Deer Valley offers and exceptional line of high-quality, full-suspension mountain bikes and helmets for rent.
Deer Valley also offers chairlift rides for sightseers and hikers. You can enjoy the spectacular scenery of the Wasatch and Uinta mountains from a comfortable, padded chairlift ride at the resort. Once at the top, you can walk down one of the main hiking trails or hike the Scenic overlook trail (a 1/4 mile route offering beautiful views down the mountain and over Jordanelle Reservoir). Those who do not want to hike down the mountain can simply reboard the left and descend.
Chairlift rides are available on both the Silver Lake Express and Wasatch Express. And adult scenic ride pass is $12; seniors 60 and over and children 6-12 years old can ride for $9. A single ride is only $6 for adults and $4 for seniors and children. Children 5 years and under ride free.
For further info about these Deer Valley adventures, call 435-649-1000 or 800-424-DEER.
The Quarry at Dinosaur National Monument has been close to the public because the building that encloses the quarry has serious structural problems. It will remain closed until renovations can be completed – probably for a period of several months.
The Quarry is the only area within the monument where the public can view dinosaur fossils embedded in rock.
Dinosaur National Monument includes a large area where people can engage in a variety of sports including hiking, camping and whitewater river running. The Quarry is the only facility that has been closed – the rest of the monument is open.
Dinosaur bones, replicas and other exhibits can be seen at several other places. In nearby Vernal, the Utah Field House of Natural History State Park showcases dinosaur fossils, life-sized replicas and other exhibits.
The Cleveland-Lloyd Dinosaur Quarry, southwest of Price, is a working quarry where the public can observe paleontological work in progress, including fossils that are being uncovered and studied.
This page lists several other places where the public and view fossils and learn about dinosaurs.
The popular Subway route in Zion National Park is now open, after having been closed in late June and early July because a wildfire threatened the area. It reopened on July 7.
All park roads are now open to the public. The following drainages, routes and trails are still completely closed until further notice: Grapevine, Coalpits Wash, Scoggins Wash, Huber Wash, Chinle Trail and Dalton Wash.
Zion Canyon, the most popular area in the park, was never threatened by the fire and remained open through the period. The Narrows, Angels Landing and other popular hikes were not affected.
A group from Utah.com hiked the Narrows recently and had a great trip. We made this video clip to showcase the hike (Flash video, 5941K).
That's how Bob Downing begins a newspaper article on mountain biking the mesa.
He goes on to say, "Gooseberry Mesa in southwest Utah near Zion National Park is gaining fans as one of the top mountain-biking spots in the United States.
"About 70 percent of the trails are over slickrock or bare Shinarump conglomerate. That is a big attraction to serious mountain bikers.
"As a Midwest biker and a slickrock rookie, I was surprised by the traction I got on the sandstone, which at first appeared to be almost unridable.
Downing writes for the Akron Beacon Journal. The article was also picked up and published by the San Luis Obispo Tribune. Read the entire article.
A unique event called Llama Fest will take place on July 15 in Spanish Fork, Utah. Llamas and enthusiasts from around the region will congregate to share information, compete for ribbons and enjoy social interaction. There will be an obstacle course, show ring, races, beautiful baby contest, crafts booths, demonstrations of spinning and weaving, food booths and other attractions. There will also be continuous performances on stage by South American bands and dance groups.
Llamas are a fundamental part of the culture in the Andes region of South America, where they are used as pack animals, wool producers and family pets. In Utah they have become very popular for carrying camping gear on treks into the Uintas and other high mountain areas. Some are also used to guard sheep herds on the open range.
Llamas are sure-footed, dependable, almost personable, and they do not cause erosion or the other environmental problems attributed to the use of horses in high country wilderness areas.
This is the 12th annual Llama Fest. The event grows in popularity every year. Activities will begin at 4 pm, on the KHQN Radio grounds on South Main in Spanish Fork. Some 4,000 to 5,000 people are expected to attend. All activities are family-friendly.
For more info see the festival website, or contact event organizers Chris or Christine Warden (chris&christine@earthlink.net).


text:
History and How It Brought Her to New Paltz's McKenna Theater: Emma Reifschneider's Story
November 24, 2020 Kerri Kolensky Features 0
Along with many theater arts students, Reifschneider frequents McKenna Theater and the Parker theater for classes, though some classes are taught online due to the COVID-19 pandemic. Photo Courtesy of Kerri Kolensky.
"Then the lights go down and we finish by screaming strike and having this really powerful moment, and then there was absolutely nothing. There was no clapping, there was no murmuring, there was nothing. Just silence."
Emma Reifschneider is right; no in-person audience witnessed her performance as Miller in the staged reading of "Waiting for Lefty" by Clifford Odets, one of SUNY New Paltz' theater productions this semester.
The audience, myself included, was at their respective homes. I watched her perform on television from my couch. There was no pre-show excitement, no waiting for the lights to drop, no rushing to settle in my chair. The broadcast started, and she appeared in the background of the opening scene, sitting in a chair and looking somewhat frazzled and unsure.
"It took me a full ten minutes to really feel like we were doing it and it wasn't rehearsal, because there was no one in the audience and usually you can't see individual faces, but you can feel their presence," said the actress.
We speak about the performance in her dormitory bedroom, a chaotic yet comforting and homey oasis nestled in a strangely quiet campus. She sits on her sky blue flowered bedspread, pillows and stuffed animals surrounding her cross-legged figure. A tapestry and string lights with clipped on photos cover her side of the wall. There are so many colors, patterns and moments captured that it's hard to know where to look.
Reifschneider bursts with energy and laughter as her hands illustrate her passions while she talks of her hometown. The college junior is a native of Stuart Manor, a Long Island town. She lives with her two parents and brother, who are not surprised by her acting aspirations. It runs in the family.
"My dad was a theater major in college and still continues to act in community theater, so I kind of caught the bug from him. And my mom's primary goal in life is to get me to do anything other than theater for the rest of my life," Reifschneider said, a joking tone evident. "But they love and support me and I love them."
Her father introduced her to theater, first taking her to a Broadway production of "The Phantom of the Opera." He took her to the audition for what would be her first performance at age nine, a local community theater production of "Meet Me in St. Louis." From there, Reifschneider performed in five of her high school's productions before coming to New Paltz and double majoring in theater and digital media management.
Since starting college, she's acted in the school's Praxis productions of "Life's Only Valuable Emotion" and "Henry IV, Part One," a staged reading. She also appeared in "Fresh Act," a student-run showcase of short plays, her freshman and sophomore year. "She Kills Monsters" during her sophomore year was her first Mainstage production and what she calls the "most rewarding."
"I was in the show as an ensemble member, but I was also an assistant director, an assistant choreographer and an understudy," Reifschneider said. "That was cool to get to wear all those different hats and experience all those different roles in the theater."
Clothed in a bright blue suit with massive padding to resemble a monstrous creature, the actress was able to use her taekwondo background in several fight scenes. She leaped and pounced throughout the entire theater, enhancing the chaos onstage.
In "Waiting for Lefty" Reifschneider stands out for different reasons. Her scene is just one of several in the production. Each character must decide what they truly value in the midst of the Great Depression while attempting to organize a labor strike. Her character, a lab worker traditionally played by a male, risks losing his job to stand up for his morals against his boss' wishes.
Reifschneider abandoned her jubilant personality during the show as her body grew more rigid and serious. The proximity of the camera gave a detailed look of her face; her eyebrows frequently furrowed in frustration at her scene partner, even with the black mask on her face. The anger only strengthened between the two characters as Reifschneider's body reflected the emotion.
She adopted a male persona, her spine rigid as she sat forward in her chair, legs wide apart and firmly planted on the floor. Even though the two actors were six feet apart, the space felt impossibly small. She demonstrated her awareness of her partner by looking anywhere but him as she reminisced about her character's deceased brother. Her command of the space was mesmerizing as she looked out into an empty theater, searching for invisible faces.
While the role and the circumstances surrounding it may have been vastly different from what she's used to, the actress said that her process in preparing for the show didn't change very much.
"I think every experience you do prepares you for something, whether you know it or not," Reifschneider said. An important part of the process for her is familiarizing herself with the material and really getting into the headspace and life of the character. "I just think about it on walks, so I'll go on runs, I think about my backstory in the shower. I think, 'where was Miller ten minutes before this scene, where was he after this scene?'"
Embodying the character and staying present is something the actress wants to improve on. "My brain never shuts up, even on the stage," she said. "If I'm in the scene it's a little bit better. I won't be thinking of that homework assignment, but I'll also be thinking, 'oh I know my grandma's watching this.'"
Reifschneider also wants to work on different types of physical movements more to bring her characters to life. "Each character that you do should have a slightly different walk," she said.
Reifschneider's future aspirations are centered around theater, though they may not involve always being on stage. While acting full time is her dream, she is also interested in producing and being a part of theater in other capacities. "I really do love the management side of things. I find it really fascinating, and I'm not just doing it because my mom told me I need a second major," she said.
The actress knows that theater will have an immense presence in her life, regardless of what she decides to do after graduation. She values the importance of theater and what it can teach others, especially during a time of turmoil in the world. "It's really hard for people to change, but people can walk out with a new perspective. I love that idea. That your work influenced someone."
kerri kolensky
new paltz theater
reifschneider


Cindy Morgan reported that those who booked rooms for the IAB Retreat should be receiving their hotel confirmations very soon.
The minutes of the 2018-02-28 tech chat and business meeting were approved.
Brian Trammell reported that the technical plenary panelists will have a conference call on 8 March 2018 to coordinate with each other.
Lee Howard and Brian Trammell took an action to update the IAB wiki to provide process guidance on organizing technical plenaries.
The IAB discussed their agenda for IETF 101.
Mat Ford will find out if Kathy Brown is available to join the IAB's Monday breakfast meeting in London.
An item on IASA 2.0 was added to the IAB's Thursday meeting agenda.
Allison Mankin reported that the budget is nearly done; she is just waiting to confirm the meeting room rental costs. Alissa Cooper suggested that since the workshop will happen in an IETF breakout room during regular session time in lieu of IRTF Research Group meetings that the meeting space should be free. Allison will follow up with the Secretariat.
In preparation for an agenda item at IETF 101 to discuss IAB Program leadership, each of the IAB Program Leads gave a brief description of their respective Programs.
More information about IAB Programs is available at <https://www.iab.org/activities/programs/>.
The IAB discussed discussed updating the IAB Statement on Identifiers and Unicode in an executive session.
The IAB discussed the ICANN Board Liaison appointment in an executive session.


Catalonia has culture-rich cities, Mediterranean beaches, soaring mountains, rivers for rafting and a whole landscape of extinct volcanic cones - all withing just a few hours' drive - or train ride - of each other. We've handpicked our Catalonia highlights on our interactive Catalonia map to help you plan your perfect itinerary, and given some sample travel times between each highlight.
One of the most relaxing things about Catalonia is that you can leave the car behind and not need to worry about driving on foreign roads or indulging in one too many post-dinner herbal liqueurs. An excellent and affordable network of trains – including shiny, new, high-speed versions – transport you away from your arrival point, leaving your tour operator to organise local transfers only. You can base yourself out of a single town or village, or cycle from place to place – arranging for your bags to be carried separately. Not only are the distances short, but the variety is immense – you can go from beach to mountains, forest to rice paddies in just a couple of hours.
This bird sanctuary is filled with hides to help you spot the many species that inhabit this thriving wetland, sitting between the estuaries of two rivers. Look out for ibis, herons, pochards, snipes and tufted ducks. Successful conservation efforts have seen the reintroduction of the white stork and the purple gallinule; visit in spring or autumn to catch sight of the migratory species.
With blue flag beaches, rugged coves, ancient villages and quaint castles, central Costa Brava lives up to its name – the Wild Coast. The industrious locals produce cheese and some of the best ceramics in Spain; the cuisine focuses on local, seasonal produce. The castle in Púbol was bought by Dalí for his wife, Gala; his curious elephant sculptures inhabit the gardens.
It's one of Europe's – if not the world's – most hyped cities, but we just can't fault Barcelona. The sun-drenched, beachside regional capital boasts vibrant markets, street performers, awesome architecture, world-class restaurants, astonishing art and nightlife to keep you entertained til dawn. It epitomises the Spanish good life, managing to be both packed with excitement yet laid back and Mediterranean.
Mainland Spain's easternmost point is a picturesque headland of crystalline bays, tumbling towns and eroded rocks that are said to have inspired Dalí's surrealist paintings; visit his house near Cadaqués, a fishing village he described as "perfect and dreamy". The Monastery of Sant Pere de Rodes is an awesome sight, and boat trips around the coast reveal colonies of monk seals.
The Ebro River flows through the medieval city of Tortosa, past quaint Horta de Sant Joan – which inspired Picasso's earliest Cubist works, and beneath mighty mountains topped with Alpine forest and swooping eagles. It empties into the Mediterranean, filtered through rice paddies. You can cycle, hike, trek up mountains, watch birds and relax on the beach – yet this region remains unknown, even to most Catalans.
In the foothills of the Pyrenees, the surreal volcanic landscape of Garrotxa is a stunning introduction to the mountains for those traveling up from the coast. The best views are from the air; hot air balloon trips can be booked to see the 40 extinct volcanic cones and lava flows from the air... The rich volcanic soil has allowed forests to flourish. Base yourself in the cultural town of Olot for easy access.
Glamourous Barcelona leaves a lot for other cities to live up to. But those who penetrate the walls of ancient Girona will find a city with plenty of charm – and none of Barcelona's crowds. The Medieval Quarter is actually a relatively "modern" district – parts of Girona date back to Roman times. The Jewish Quarter is one of the most picturesque; visit the Ramblas, market places and cafes for a true taste of urban Catalonia.
Montserrat Monastery is a site of pilgrimage for Catalans as well as tourists. It sits almost at the top of a 1,236m high mountain, standing guard over the surrounding lowland plains. The cable car ride may seem like the easy option, but it's still stomach-churningly high! If that's not enough, you can hike the surrounding peaks – be sure to take a map. As well as its impressive location, Montserrat is famous for its Black Madonnas.
Just a short drive from the Tarragona coast, the strange form of the Sierra del Montsant feels like another world. The foothills 'Sacred Mountains' conceal the ruins of the 12th century monastery of Scala Dei, where monks cultivated crops on the steep mountainsides for centuries. Guided walks in the mountains reveal a wealth of biodiversity in this well preserves park, or trek to the peaks, which reach up to 1,163m.
Outdoor adventurers should head to this sparsely populated region. The Nogueres Pallaresa River is the hub of many activities here, including whitewater rafting, kayaking and swimming – as well as abseiling and canyoning down the canyon walls. There are hiking, mountain biking and horse riding trails for all abilities; the small town of Sort makes an excellent base, especially during its July festival.
In the Costa Brava's northernmost region of Alt Empordà, this picturesque little village is sandwiched between countryside and coast, on the banks of the River Fluvià. Nature trails explore these varied landscapes and the birds that inhabit them, while the flat scenery lends itself to gentle bike rides. Take a detour to St Pere beach, which has 6km of sand dunes; windsurfers sail offshore.
A historical city backing onto a beach, a Roman coliseum alongside tapas-bar filled plazas, Tarragona is a city for unwinding and unravelling, as you stroll through the ancient streets. The many Roman ruins are a UNESCO site; for livelier sights come and see the human castell towers being built, or the firework festival each July.
The following times give you a rough idea of the driving times between the main attractions in Catalonia.


text:
Q: Calculating the Fenchel Conjugate I know this might seem as a simple question, but I just hope that I can learn how would people normally approach this question? Thanks in advance!
Compute the Fenchel conjugate of the following function:
$f(x) = e^x, x \in \Bbb R$
The Fenchel conjugate is defined as:
$f^*(x^*) = sup\{\langle x, x^*\rangle - f(x)\}$

A: This is a real function, so the inner product here is simply multiplication. You need to find
$$f^*(y) = \sup_{x \in \Bbb{R}} yx - f(x) = \sup_{x \in \Bbb{R}} yx - e^x.$$
This is a relatively simple optimisation problem. We have this differentiable function of $x$, with some fixed unknown $y$, and we want to find the maximum value of this function.
First, let's analyse the stationary points. We have, when differentiating (partially) with respect to $x$ and setting to $0$,
$$y - e^x = 0 \implies x = \ln y,$$
when $y > 0$. So, in this case, we get one stationary point at $x = \ln(y)$, producing a possible maximum of
$$y\ln(y) - e^{\ln(y)} = y \ln y - y.$$
We just need to compare this with the limits as $x \to \pm\infty$. As $x \to \infty$, then $yx - e^x \to -\infty$, regardless of the value of $y > 0$. As $x \to -\infty$, again assuming $y > 0$, we have $yx - e^x \to -\infty$ as well. Thus, the maximum must occur at the one and only stationary point, implying,
$$f^*(y) = y\ln(y) - y$$
when $y > 0$.
If $y \le 0$, then $y - e^x < 0$ for all $x$. This means that the function $yx - e^x$ is strictly decreasing in $x$, and hence the supremum is the limit as $x \to -\infty$. If $y < 0$, this limit is $\infty$. If $y = 0$, then the limit is $0$. So, our full conjugate is
$$f(y) = \begin{cases} y \ln(y) - y & \text{if } y > 0 \\ 0 & \text{if } y = 0 \\ \infty & \text{if } y < 0. \end{cases}$$


text:
\section[]{Introduction}
\label{sec:intro}

The impact of an active galactic nucleus (AGN) on its host galaxy and
their wider surroundings was not appreciated until relatively recently
\citep[e.g.][]{bower06,croton06}. The role of AGN feedback in the
formation, evolution, and environment of the most {\it massive}
galaxies is particularly important, given the larger mass of the
central black hole and the denser surrounding gas halo of
these systems, see \citet{mcnamara12} and \citet{fabian12} for recent
reviews.

The prototypical example of AGN feedback within a cluster of galaxies
can be found in the Perseus cluster \citep{bohringer93,fabian01}, host
to the active brightest cluster galaxy (BCG) NGC\,1275. The spectral
properties of the nuclear narrow-line radio source 3C\,84 place it as
intermediate between a BL Lac object and a Seyfert
galaxy. Significantly, NGC\,1275 is one of the very few sources
detected by the {\it Fermi Gamma-ray Space Telescope} (hereafter {\it
  Fermi}), that is not strongly beamed \citep{abdo09a}, and exhibits
pronounced flaring activity \citep[see][]{kataoka10,brown12}.  During
these high-energy (HE) flares, the source becomes significantly harder
\citep{brown12}, and bright enough to detect in TeV $\gamma$~rays
\citep{aleksic12}. The magnitude of the variability in the HE regime
is much greater than that observed in other {\it Fermi}-detected radio
galaxies (e.g. Centaurus-A and M\,87).  Given this, and given the
small sample of such sources, and the fact that NGC\,1275 is the most
massive of these galaxies, particular attention is warranted.

It has been postulated that the central AGN comprises a viscous
accretion disk tilted with respect to the rotating (Kerr)
super-massive black hole, bringing about precessing jets as a result
of torques acting on the disk \citep{falceto10b}. This then accounts
for the observed `S-shaped' morphology of the radio jets, which are
seen to expand into lobes tens of kiloparsecs in extent. Based on
infra-red observations of circumnuclear molecular gas, kinematic
arguments imply a black hole mass of $3.4\times10^{8}$\Msol
\citep{wilman05}. An inherent uncertainty in this value arises from
not knowing the system's true inclination to our line of sight.  Very
Long Baseline Interferometry (VLBI) maps of 3C\,84 can place
constraints on this, suggesting that the milli-arcsecond jet is at
$\leq14.4$\degr~to the observer's line of sight
\citep{krichbaum92}. Closer to the core the constraint is more
stringent ($\theta\leq2.7$\degr), whereas on arcsecond scales the
angle is 39.4\degr$\leq\theta\leq$58.2\degr. For such conditions to be
satisfied, there must be some curvature of the jet away from the line
of sight \citep{dunn06}. \citet{suzuki12} identify new jet components
in the core of NGC\,1275 from Very Long Baseline Array (VLBA) 43\,GHz
imaging, that appear between 2002 and late 2008 and show that the
majority of the increase in flux density at this frequency is due to
the innermost two components. \citet{aleksic13} show that for one of
these VLBA components (`C3'), this value almost doubled between the
end of 2009 and the start of 2011, which can account for the entirety
of the single dish flux increase over this period. Curiously, both
\citet{nagai10} and \citet{suzuki12} claim that C3 is moving relative
to C1, as the latter was in the earliest VLBA observations in
2002. However, an alternative interpretation of these observations is
that C3 is coincident with the nucleus of the galaxy but was
undetected before 2003 due to its inactivity.  We will return to this
point in Section~\ref{ssec:current-outburst}. The core is also known
to vary significantly on short timescales at optical
wavelengths. \citet{kingham79} detected variability of in excess of 30
per cent on timescales of months. Similarly, \citet{lyutyi77} found
variations of 0.2\,mag on 10--20 day timescales. \citet{nesterov95}
show evidence that this optical variability is only observed until
1980.

Observations in the X-ray waveband reveal cavities that anti-correlate
with the radio features, leading to the conclusion that the central
engine is able, through its jets, to inflate bubbles of hot,
relativistic plasma into the surrounding thermal gas of the
intracluster medium (ICM), displacing it. Further evidence to support
this includes the additional X-ray cavities to the north-west and
south of the core, where the the radio lobes have detached and risen
buoyantly through the ICM, forming `ghost bubbles'.  Indeed, the
northern bubble has been likened in appearance to a spherical cap air
bubble rising in water \citep{fabian03b}. The position of the
older generation of X-ray cavities with respect to the younger,
radio-active pair is misaligned, suggesting that the detachment
occurred at a different phase in the cycle of jet precession. The
observed X-ray and radio emission can be produced by a precession
period, $\tau_{{\rm prec}}$ of $3.3 \times 10^{7} {\rm yr}$, an
opening angle of 50\degr, and an inclination of the precession axis to
the line of sight of 120\degr~\citep{dunn06}.

On larger scales, Perseus hosts a $\sim$300\,kpc radio mini-halo
centred on NGC\,1275, with spectral steepening away from the cluster
core. It has been proposed that the energy required for the particle
acceleration is provided by magnetohydrodynamic (MHD) turbulence in
the cooling flow \citep{gitti02}.

Another feature observed in NGC\,1275 is a spectacular optical
nebulosity: a filamentary system of ionised, H$\alpha$-emitting gas
extending over 100\,kpc \citep{fabian03a}. Both radial and tangential
filaments are seen, the latter curving around the galaxy
\citep{conselice01}, and the brighter features are also detected in
the soft X-rays. It has been suggested that they reveal the flow of
the hot gas of the rising radio bubbles. An example of such a tracing
streamline is the `horseshoe'-shaped filament, which clearly turns
back on itself at the boundary of the outer buoyant bubble. One
interpretation then, is that the bubble draws the ionised gas into its
wake as it rises \citep{fabian03b}, and there is enhanced cooling
along its edge, where the ICM is compressed.

The need for a feedback mechanism within the Perseus system to
counteract the cooling flow was identified with such measurements as
the temperature of intracluster gas, which has been found to be above
a third of the virial temperature, given that the ICM has a short
cooling time on the galactic scale \citep{salome06}. The coincidence
of X-ray cavities with the radio lobes of NGC\,1275 is evidence that
the central source can suppress gas cooling. Mechanical feedback from
the AGN, with an energy output estimated to be $\approx
10^{43}$\,erg\,s$^{-1}$, is able to contribute toward this re-heating
effect \citep[see e.g.][]{fabian94}. Whether some additional source of
heating is also necessary to produce the observed suppression is
highly debated. Critically, the AGN output of NGC\,1275 is variable on
decade-long timescales. \citet{odea84} show that NGC\,1275 varied
substantially over the 22 years between 1960 and 1982 at
2--100\,GHz. \citet{abdo09a} note that the 15\,GHz flux density of
NGC\,1275 declined dramatically between 1982 and 2005, but has
increased steadily since then. They also observe that these changes in
radio output are mirrored in the $\gamma$~rays. It is this connection that
we investigate in more detail in this paper.

We begin by describing our analysis procedure in
Section~\ref{sec:analysis}. Our results are presented in
Section~\ref{sec:results} and discussed in
Section~\ref{sec:discussion}, with a focus on the connection between
the non-thermal sub-millimetre emission and the gamma radiation,
including a review of the historical activity of the
source. Conclusions are then drawn and prospects suggested in
Section~\ref{sec:conclusion}.

\section[]{Observations and Data Analysis}
\label{sec:analysis}

On board the {\it Fermi } spacecraft is the Large Area Telescope (LAT): a
pair conversion instrument sensitive to high-energy photons
($\sim$\,20 MeV --\,$>$300 GeV) with a large effective area and wide
field of view (2.4 sr, and $\sim$\,6500\,cm$^{2}$ on-axis at 1\,GeV
based on post-launch instrument response functions (IRFs),
respectively). A detailed description of the detector is given in
\citet{atwood09} and references therein, and a post-launch review of
its in-flight performance and the IRFs in
\citet{ackermann12}. Primarily, observations are made when the {\it Fermi }
satellite is in {\it sky survey mode}, i.e. the spacecraft is pointed at
some angle from the zenith and rocked about its orbital plane, north
for one orbit then south for the next, providing uniform sky exposure
on a $\sim$3-hour cycle.

Reprocessed {\it sky survey mode} event and spacecraft data amassed
between the 4$^{th}$ of August 2008 (the date after which
science-data-taking began) and the 6$^{th}$ of March 2014 (a
Mission-Elapsed-Time interval of 239557417 to 415756803, equating to
$\sim$2039 days) were extracted for a source region (SR) of
20\degr~centred on the position of NGC\,1275 (RA =49.951\degr,
Dec. =$+41.512$\degr; taken from data in the literature) and in the
energy range $300\,{\rm MeV} \leq E \leq 300\,{\rm GeV}$, which
excludes events at the lowest energies visible to {\it Fermi }, where the
high point spread function (PSF) leads to considerable source
confusion. A zenith cut of 100\degr~was applied to exclude HE photons
from the Earth's limb, and all `Source' class events were
accepted. The data were analysed using the {\it Fermi } Science Tools
version v9r32p5, and IRF P7REP$\_$SOURCE$\_$V15.

A binned, point-source analysis of NGC\,1275 was carried out. Data
were fitted to a source model constructed to encompass emission from
local (that is, within the SR) sources listed in the {\it Fermi}-LAT  Second
Source Catalog (2FGL; \citealt{nolan12}), the diffuse Galactic and
extragalactic (isotropic) $\gamma$-ray backgrounds (recent models
gll\_iem\_v05.fits and iso\_source\_v05.txt
respectively\footnote{http://fermi.gsfc.nasa.gov/ssc/data/access/lat/BackgroundModels.html}
were used; their normalisation free to vary) and the candidate source
itself. The photon index and normalisation for objects within
1\degr~of NGC\,1275 were allowed to vary. Outside of this region but
within the specified {\it region of interest} (ROI) of 10\degr, the
normalisation was free to vary, but the photon index was fixed to the
2FGL value. Sources outside of the ROI but within the SR were included
in the model, but both aforementioned parameters were fixed to the
catalogue values.

The maximum-likelihood spectral estimator {\sc gtlike} was used to
perform a {\it binned} fit, modelling the source emission with a power
law spectrum. {\sc gtmodel} was then used to obtain a model map of the
region given the result of the fit. {\sc gtbin} was utilised to
construct a counts map from the data, and a binned exposure cube was
generated (through use of the {\sc gtexpcube2} tool) as part of the
binned likelihood analysis chain. A binned method of likelihood
fitting was adopted over an unbinned one, because it has been found to
be more robust. The fit outputs a Test Statistic for the source, a
spectral index and an integrated flux.

{\sc gtbin} was also used to construct source light curves through
aperture photometry. Monthly, fortnightly, and 3.5-day binning
was applied to the data, within an ROI of 1\degr. The background was
estimated in two manners: firstly, the model-predicted source flux
contained therein was subtracted from the overall model-predicted
flux, calculated by integrating over the ROI in the corresponding
model map given weighted exposure maps across thirty bins in
energy. This value was then multiplied by a correction factor to
account for the tails of the PSF that lie outside the aperture
selected for the light curve, which was estimated by taking the ratio
of the average exposure across all time bins for the light
curve-specific ROI and the larger region used to perform the
likelihood fit, calculated using the {\sc gtexposure} tool. Secondly a
`mean background' light curve was constructed by averaging the flux
within a pair of {\it off-source} regions in the field (at equal
Galactic latitudes to NGC\,1275, and containing no 2FGL sources)
binwise. Subtracting either of these backgrounds from the raw flux in
each bin gives an estimate of the relative excess from the source, and
allows for comparison between model-dependent and independent measures
of the flux level.

The data were divided into two bands in energy (a `low' cut below 3
GeV, and a `high' cut above 3 GeV) and the initial analyses repeated
in an otherwise identical manner. The ROI selected for constructing
light curves in these bands was based on the LAT PSF at the lower
energy bound (0.4\degr\ for the high band; 2.3\degr\ for the low band)
in an effort to conserve all available source photons. The evolution
of hardness ratio (HR) was investigated by dividing the high-band
excess flux by that of the low-band, binwise. The HR was also plotted
against the monthly source flux across the full energy range.

The historical radio data have been collated from a number of
different studies and observatories. The 14.5\,GHz University of
Michigan Radio Astronomy Observatory (UMRAO) monitoring of NGC\,1275
is presented in \citet{abdo09a} and we refer the reader to this paper
and the excellent historical record that the UMRAO project provides
for this source (and many others) for the 4.8, 8.0 and 14.5\,GHz
light curve of NGC\,1275. Our emphasis in this work is the
higher-frequency ($>$20\,GHz) data where the coverage is less
coherent. \citet{odea84} present the best pre-1980 light curve of
NGC\,1275, to which we have added the Mets\"ahovi data
\citep{nesterov95} at 32--37\,GHz and 90\,GHz. We also extract
photometric points from \citet{schorn68}, \citet{hobbs69},
\citet{fogarty71}, \citet{epstein79}, \citet{landau80},
\citet{flett81,flett83}, \citet{barvainis84}, \citet{steppe93},
\citet{reuter97}, and \citet{nagai12}, at both of these frequencies.  We
include yearly averages of the 85--95\,GHz fluxes from
\citet{trippe11} in the period between 1996--2010, which are a subset
of the data presented in that paper.

The flat spectral index of the source at 30--40\,GHz means that the
differences between 32 and 37\,GHz observations are relatively small,
and are swamped by the order-of-magnitude change seen over the last 50
years.

Finally, we include Wilkinson Microwave Anisotropy Probe ({\it WMAP})
and {\it Planck} 33/30 and 94/100\,GHz data, respectively
\citep{wright09,planck11} to show the most recent fluxes averaged over
each of the nine years of the {\it WMAP} mission (August 2001 to
August 2010), and the first 15 months of {\it Planck} operations
(August 2009 to November 2010).

\begin{figure*}
  \centering
  \includegraphics[width=16cm]{./NGC1275_MW.eps}
  \caption{The {\it Fermi } light curve for NGC\,1275 since launch (August
    2008), between 300\,MeV and 300\,GeV and within 1\degr, with
    fortnightly binning. The model-predicted background level is
    indicated, and has been subtracted from the raw flux to produce
    the source light curve. Overlaid is the SMA calibrator monitoring
    data at 1.3\,mm. }
  \label{fig:1}
\end{figure*}

We also make use of 1.3\,mm data from the Submillimeter Array (SMA)
calibrator monitoring, to provide a more detailed flux comparison
since the launch of {\it Fermi}, as it has the largest number of
available datapoints. \citet{gurwell07} describe the SMA Phase
Calibrator monitoring in detail. NGC\,1275/3C\,84 has been observed
regularly from the start of SMA operations in late 2002 at 1.3\,mm and
870\,$\mu$m. Save for gaps between March and May each year when the
source is a daytime object, the time coverage is relatively uniform
with typically several observations per week, see Fig.~\ref{fig:1}. We
use all the available data within a frequency range 220--230\,GHz to
ensure the fluxes are comparable. The SMA observations are made at a
variety of baseline configurations, so some flux could be resolved out
at the longest baselines. However, given the radio structure at lower
frequencies, the fraction of the 1.3\,mm continuum that comes from
scales larger than $\sim$2\arcsec~is likely to be small even when the
source is at its weakest. Therefore the SMA flux should be unaffected
by the configuration and any increase can be attributed to flux from
the unresolved core component. This selection makes use of over 80 per
cent of the 1.3\,mm SMA datapoints, as there is a strong preference
for this narrow frequency range from SMA observers.

\section[]{Results}
\label{sec:results}

\begin{figure*}
  \begin{center}
    \subfigure{%
      \includegraphics[width=15cm]{./NGC1275_MW_zoom1.eps}}\\
    \subfigure{%
      \includegraphics[width=15cm]{./NGC1275_MW_zoom2.eps}}\\
    \subfigure{%
      \includegraphics[width=15cm]{./NGC1275_MW_zoom3.eps}}
  \end{center}
  \caption{Detailed {\it Fermi } light curves for NGC\,1275, between
    300\,MeV and 300\,GeV and within 1\degr, focusing on ({\bf top})
    the 2009--2010 period, ({\bf middle}) the 2010--2012 period, and
    ({\bf bottom}) the 2012--2014 period, with 3.5-day binning,
    overlaid with SMA calibrator monitoring data at 1.3\,mm.}
  \label{fig:2}
\end{figure*}

The point-source binned likelihood analysis of NGC\,1275 between the
4$^{th}$ of August 2008 and the 6$^{th}$ of March 2014 outputs an
integrated flux between 300\,MeV and 300\,GeV of
(7.62$\pm$0.10)$\times 10^{-8}$ ph\,cm$^{-2}$s$^{-1}$, a photon index
of 2.141$\pm$0.003, and a Test Statistic of $\sim$27350 (equivalent to a
detection significance of $\sim$165$\sigma$, see \citealp{mattox96}),
where errors are statistical only. Fig.~\ref{fig:1} shows the
fortnightly-binned {\it Fermi } light curve for NGC\,1275 over this time
period, together with the model-predicted background flux within the
ROI, and overlaid with the SMA calibrator monitoring data at
1.3\,mm. In the latter, there are several small brightenings
($\sim$\,25--30 per cent) on 1--2 month timescales, but none
comparable to the amplitude observed in 1965--1980 as yet. From the
{\it Fermi } light curve, a number of `flares' may be identified, the
earliest of which are discussed in \citet{brown12} and
\citet{kataoka10}. An overall trend of increasing baseline flux is
seen in both datasets.

Fig.~\ref{fig:2} comprises a series of finer (3.5-day binning) {\it Fermi }
light curves for NGC\,1275, detailing the 2009--2010, 2010--2012, and
2012--2014 periods (each of which contain prominent flares visible in
the fortnightly-binned light curve), and again overlaid with the SMA
calibrator monitoring data at 1.3\,mm. Though the statistics are poor,
these light curves illustrate the erratic nature of the HE flux level,
highlighting the differing patterns in each flaring event, and
features such as the drop in emission to near-background level in
early 2011 (also apparent in Fig.~\ref{fig:1}).

Fig.~\ref{fig:3a} is a plot of the HR against time with monthly
binning, with the source light curve (binned likewise) included for
comparison. The possibility of correlation between HR and flux is
investigated in Fig.~\ref{fig:3b}, which shows the HR plotted against
the integrated flux for the full energy range. Observing harder
emission during brighter periods is in agreement with
\citet{brown12}. There is indeed a hint that during the brightest
months, the corresponding HR is higher, however this correlation is
stronger earlier on, as illustrated by dividing the data into two time
periods: In the thirty-five months following launch, the correlation
factor is 0.53, compared with 0.28 after this epoch, evidencing a
deviation from the established {\it harder-when-brighter} behaviour at
later times.

\begin{figure*}
  \begin{center}
    \subfigure[][{\label{fig:3a}}]{%
      \includegraphics[width=8cm]{./NGC1275_hr_1month.eps}}
    \subfigure[][{\label{fig:3b}}]{%
      \includegraphics[width=8cm]{./NGC1275_hrVflux_1month.eps}}
  \end{center}
  \caption{A plot of the hardness ratio (defined in
    Section~\ref{sec:analysis}; derived from `high' and `low'-energy
    band data) against time for NGC\,1275, with monthly binning (a),
    and HR plotted against the $\gamma$-ray integrated flux for the full
    energy range for NGC\,1275 (b), with points divided into two time
    periods: prior to (in red) and following (in black) an apparent
    increase in the degree of correlation, as indicated by the dashed
    red line in (a).}
 \label{fig:3}
\end{figure*}

The light curve-specific ROI does contain another point source of HE
emission (associated with the radio galaxy IC\,310), and this cannot
be easily removed from the light curve, as the emission is barely
resolved from that of NGC\,1275. The background-subtracted light curve
may be very slightly overestimated as a result, but the model, which
considers a larger ROI and SR, does include this source. Likewise
there are several 2FGL sources in the ROI and SR, but these are
included in the model. The two methods of background estimation are in
agreement within the errors associated with the mean background light
curve, which may be fit with a polynomial of order zero, $F_{\gamma} =
(2.50 \pm 0.04)\times 10^{-8}$\,ph\,cm$^{-2}$s$^{-1}$, whilst the
model-predicted background level is $F_{\gamma} = 1.21 \times
10^{-8}$\,ph\,cm$^{-2}$s$^{-1}$. The choice of background estimate
does not very appreciably affect the trend observed in
Fig.~\ref{fig:3b}. A correlation was sought binwise between the
model-subtracted source flux, and the difference between the two
background estimates, but not found, rejecting the hypothesis that
photons from the PSF tail of NGC\,1275 might be contributing
significantly to the flux in the off-regions.  The model-predicted
background was adopted throughout the work presented here, for
consistency within the analysis chain. The aperture correction factor
applied to this background estimate as described in
Section~\ref{sec:analysis} was 1.74 for the overall 300\,MeV$\leq E
\leq$300\,GeV band; 1.32 for the high band and 1.25 for the low band.

\section[]{Discussion}
\label{sec:discussion}

\subsection[]{Historical Consideration}
\label{ssec:history}

\begin{figure*}
  \centering
  \includegraphics[width=16cm]{./NGC1275_historicalMW.eps}
  \caption{An historical light curve for NGC\,1275. A flux above
    100\,MeV is derived for the emission noted in the {\it COS B} data
    in the direction of the cluster. The EGRET upper limit on the flux
    from Perseus is included, and yearly fluxes for NGC\,1275 as
    observed using the {\it Fermi }-LAT. Collected archival radio data
    (described in Section~\ref{sec:analysis} above) is also included,
    at 90 and 32--37\,GHz.}
  \label{fig:4}
\end{figure*}

Historically, NGC\,1275 is a highly-variable source of non-thermal
radiation, strongly motivating its investigation with {\it Fermi}, and
particularly suggestive of a relationship between the HE and radio
emission. Whilst both leptonic and hadronic scenarios are possible for
the $\gamma$-ray emission from NGC 1275, we focus in the following on the
most common interpretation of this emission as inverse Compton
scattering of a relativistic electron population, which is also
responsible for the synchrotron emission seen at radio-mm wavelengths.

The European Space Agency (ESA)'s {\it COS B} mission in the late
1970s \citep{bignami75} revealed an excess of HE emission toward
Perseus ($F_{\gamma}=8.3\times10^{-7}\,{\rm ph}\left (> 70\,{\rm MeV}
\right ){\rm cm}^{-2}{\rm s}^{-1}$; positional uncertainties were not
given), which was interpreted as evidence that NGC\,1275 is a $\gamma$-ray
source \citep[see e.g.][]{strong83}, however the galaxy was not
detected using the National Aeronautics and Space Administration
(NASA)'s Energetic Gamma Ray Experiment Telescope (EGRET) on board the
{\it Compton Gamma-ray Observatory} ({\it CGRO}), which flew
throughout the 1990s. A $2\sigma$ upper limit for the Perseus cluster
of $F_{\gamma} < 3.72 \times 10^{-8}\,{\rm ph}\left (> 100\,{\rm MeV}
\right ){\rm cm}^{-2}{\rm s}^{-1}$ was given
\citep{reimer03}. Contrariwise, NGC\,1275 is firmly-detected using the
      {\it current}-generation {\it Fermi } \citep{abdo09a}, and in 2010 was
      detected above 100\,GeV using the Major Atmospheric Gamma
      Imaging Cherenkov (MAGIC) telescopes \citep{aleksic12},
      establishing the source as a VHE emitter. As noted by
      \cite{abdo09a}, the $\gamma$-ray variability of the source matches
      that of the higher-frequency radio emission from the UMRAO
      15\,GHz monitoring. We extend this analysis to 30 and 90\,GHz
      over the past $\sim$50 years, and find that the long-timescale
      variation of both the $\gamma$-ray and millimetre emission are
      related. As shown in Fig.~\ref{fig:1} the connection between
      these two components on shorter timescales is not as
      well-correlated, but this is to be expected if the millimetre
      emission is strongly synchrotron self-absorbed early in any
      flaring event.

Combining all of the archival radio data produces 32--37\,GHz and
90\,GHz light curves that show a dramatic variation over the past
$\sim$50 years, as seen in Fig.~\ref{fig:4}. The scatter in photometry
at both frequencies before 1978 may in part be due to the difficulty
in determining accurate fluxes, but could also be related to a period
of enhanced variability, or `flickering', due to larger variations in
accretion during outburst. Interestingly, \citet{nesterov95} note this
period of strong variability in the radio and optical, and speculate
that it is related to the structure of the jet. Taking the period in
which there is significant optical variability as 1965--1980 (from
fig.~1 in \citealt{nesterov95}), the dramatic declines at 90\,GHz and
then at 35\,GHz follow 1--3 and 7--8 years after this,
respectively. Given the increasing time lag seen in the data at lower
frequencies due to synchrotron self-absorption, it may be that the
very gradual decline at $<$100\,GHz is a combination of the many
individual components formed before the 1980 brightening at lower
frequencies, before fading as they move away from the core and become
less self-absorbed.

\begin{figure}
  \centering
  \includegraphics[width=8cm]{./NGC1275_index.eps}
  \caption{A plot of the average spectral index of NGC\,1275, $\alpha$
    between 35 and 90\,GHz, against time, where the flux is
    proportional to $\nu^{\alpha}$}
  \label{fig:5}
\end{figure}

We have determined the average spectral index between 35 and 90\,GHz
for the period during which the two high frequency light curves
overlap, and show in Fig.~\ref{fig:5} how this spectral index changes
over time. The dramatic transition between the period prior to 1980,
and the 1990--2000 interval, where the spectral index falls from 0.0
to -1.0, is strongly suggestive of a cessation of activity in the core
around 1980, in line with the aforementioned lack of significant
optical variability after that point. The timescale for this change in
spectral index is related to the strength of the synchrotron
self-absorption at different frequencies.

Fig.~\ref{fig:6} shows the yearly-averaged {\it WMAP} and {\it Planck}
light curves for the source, and the radio-to-far-infrared spectral
energy distribution (SED) for 2002 and 2010, including points from the
UMRAO monitoring \citep{aller85}, and the literature, to show the
spectral variation at high frequencies ($>$5\,GHz) during this period,
as the flux begins to rise. In particular, note that the 4.8\,GHz
UMRAO flux falls between 2002 and 2010 compared to the increase seen
at all other frequencies.

\begin{figure*}
  \begin{center}
    \subfigure[][{\label{fig:6a}}]{%
      \includegraphics[width=8cm]{./NGC1275_planck.eps}}
    \subfigure[][{\label{fig:6b}}]{%
      \includegraphics[width=8cm]{./NGC1275_planck_sed.eps}}
  \end{center}
  \caption{Plots showing a recent yearly-averaged light curve (a) and
    the radio-to-far-infrared spectral energy distribution (b) for
    NGC\,1275, using data from {\it WMAP}, {\it Planck}, UMRAO
    monitoring, and the literature.}
 \label{fig:6}
\end{figure*}

\subsection[]{Current Outburst}
\label{ssec:current-outburst}

The increase in high-frequency radio and $\gamma$-ray emission from
NGC\,1275, coupled with the change in the spectral index after
$\sim$2002 implies that the source has become active again. The two
epochs in Fig.~\ref{fig:6b} coincide with a minimum in the radio flux,
and a point well into the current outburst, respectively. Importantly,
they mark the start of the {\it WMAP} mission in 2002, and the start
of the {\it Planck} survey in 2009. The well-calibrated photometry,
particularly for {\it Planck}, allows us to determine the spectral
index well above the peak induced by the synchrotron
self-absorption. The most recent data show that the spectral
flattening seen in Fig.~\ref{fig:6b} is related to power law emission
that extends into the far-infrared, and that the core has a more
pronounced GHz-peaked spectrum, with a peak frequency of $\sim$15\,GHz
in 2010.

The complex changes evident from the multi-frequency properties of
NGC\,1275 during the last outburst emphasise how vital regular
monitoring over a wide frequency range (particularly in the mm/sub-mm)
is, if we are to understand the processes that generate this
emission. Fortunately over the past decade, the source has been
regularly observed as part of the F-GAMMA program \citep{angelakis12}
and the Owens Valley Radio Observatory (OVRO) 40\,m Telescope
Monitoring Program \citep{richards11}, and is used as a bright phase
calibrator or pointing source at mm/sub-mm wavelengths by the Institut
de Radioastronomie Millimetrique (IRAM)'s Plateau de Bure
Interferometer (PdBI) \citep{trippe10}, the James Clerk Maxwell
Telescope (JCMT), the SMA, and the Combined Array for Research in
Millimeter-wave Astronomy (CARMA). Therefore, it is very likely that a
well-sampled light curve will be available over the 15--350\,GHz range
to search for any flickering and correlation with the optical and/or
$\gamma$-ray emission.

To illustrate the potential of combining mm/sub-mm monitoring with the
$\gamma$-ray emission we compare the SMA 1.3\,mm data to the fortnightly-
and 3.5-day-binned {\it Fermi } light curves (Fig.~\ref{fig:1}
and~\ref{fig:2}). As stated above, the variations at 1.3\,mm do not
coincide with the flares in the {\it Fermi } data. Notwithstanding, we
perform a cross-correlation to search for any linear relation between
the two datasets displayed in Fig.~\ref{fig:1}. As the SMA data are
unevenly sampled, we use the Discrete Correlation Function
\citep[DCF;][]{edelson88}. The DCF is only applicable to stationary
data \citep[e.g.][]{welsh99} so a first-order polynomial was first
fitted to, and subtracted from each dataset, in order to remove the
long-timescale, rising trend. The DCF for a range of
-1500$<$lag$<$1500 days is shown in Fig.~\ref{fig:7}. A 30-day DCF bin
width was used (it being larger than the mean sampling rate of the
$\gamma$-ray data of $\sim$15 days), giving a minimum of 110 time lag
estimates in each bin. To assess the significance of any peaks in the
DCF we use the Bartlett formula \citep{bartlett48} to estimate the 95
and 99 per cent confidence intervals, as included in the figure. The
most significant features in the data are a positive correlation at
$\sim +$800 days, as well as a negative correlation seen at $\sim
+$1100 days. A positive correlation is also seen at $\sim -450$
days. Using a DCF bin size of 100 days, the peaks in the DCF are still
present above the 99 per cent level. However, we note that the peaks
in the DCF can arise from the underlying shape of uncorrelated
coloured-noise light curves \citep[e.g.][]{alston13}. Also, removing
both the broad, 5-month peak at the end of 2011 from the HE dataset,
and the 2-month peak in early 2013 from the SMA dataset causes the
sub-mm lag to disappear, which might suggest it is spurious.

\begin{figure}
  \centering
  \includegraphics[width=7cm]{./NGC1275_dcf.eps}
  \caption{A plot of the DCF produced by cross-correlating the {\it Fermi }
    and SMA light curves shown in Fig.~\ref{fig:1}. The 95 and 99 per
    cent confidence intervals estimated using the Bartlett formula
    \citep{bartlett48} are included, though we note that they do not
    include the effect of uncorrelated coloured noise
    \citep[e.g.][]{moerbeck13}.}
  \label{fig:7}
\end{figure}

The finely-binned light curve illustrated in Fig.~\ref{fig:2} is
suggestive of significant variability on timescales shorter than the
fortnightly binning shown in Fig.~\ref{fig:1}. The possibility of a
flickering nature of the $\gamma$-ray emission is an aspect of the source
that could be used to determine its structure, and so it was
investigated further. We performed chi-square tests with the
variously-binned datasets to determine the scale down to which there
is evidence of variability. Though we found no evidence for
statistically significant variability on the 3.5 day timescale in the
{\it overall} dataset, we found hints of such during shorter,
individual periods. For example, we calculated $\chi^{2}=1.25$ per
degree of freedom for the interval illustrated in the middle panel of
Fig.~\ref{fig:2}, implying a chance probability of consistency with
the trend observed in the fortnightly-binned data of $\sim$1 per cent
It is this period (2010--2012) which contains one of the most
prominent flares. It is clear that on the timescales probed in
Fig.~\ref{fig:2}, evidence for variations from one half-a-week to
another (that do not simply reflect the variability observed in
Fig.~\ref{fig:1}) begins to emerge in some periods, in spite of poor
statistics.

The source of variable high energy $\gamma$~rays is coincident (within
errors), with the nucleus of NGC\,1275. Light-crossing-time arguments
(which state that emitting regions can only fluctuate over a time less
than that taken for light to travel across their extent) mean that any
flux variability observed limits the physical size of (at least some
component of) the source emission. The detection of a $\gamma$-ray flare
by {\it Fermi } on timescales of days to weeks places a firm upper limit on
the size of the $\gamma$-ray emitting region of less than about
1000\,AU. On the other hand, the SMA 1.3\,mm monitoring does not show
any strong variation on timescales of less than a week, so this
emission is either self-absorbed, or from a more extended region. The
EGRET upper limit of $F_{\gamma} < 3.72 \times 10^{-8}\,{\rm ph}\left
(> 100\,{\rm MeV} \right ){\rm cm}^{-2}{\rm s}^{-1}$ provides a limit
on the cluster-scale $\gamma$-ray emission of Perseus, which is expected
for example from diffuse populations of long-lived CR hadrons
\citep[see e.g.][]{blasi07}, and in models of dark matter annihilation
\citep[e.g.][]{bringmann12}. Even the lowest flux states evident in
Fig.~\ref{fig:1} are an order of magnitude above this level.

As mentioned in the introduction, 43\,GHz VLBA monitoring of NGC\,1275
shows that one component, `C3', accounts for most of the increase in
the total flux at this frequency
\citep{nagai10,suzuki12,nagai12,aleksic13}. If one assumes that C3 is
coincident with the nucleus then the evolution of the separation
between C1 and C3 presented in \citet{nagai10} and \citet{suzuki12}
can be interpreted as C1 being launched from the nucleus between 2001
and 2003. This coincides with the upturn in activity in the radio and
is a more natural explanation than a rapid change in the apparent
speed of C3 \citep{nagai10}, but implies that the flat spectrum of C1
between 22 and 43\,GHz is not due to it being the core as assumed by
\citet{suzuki12}. This indicates that new VLBA components from flaring
activity in 2010 and 2011 should become visible in the next couple of
years close to C3, and move north if they share the same apparent
velocity as C1 relative to the core. Continued VLBA monitoring of
NGC\,1275 will clarify this issue as it will allow us to link the
complex photometric variations to individual resolved knots.

The lack of any significant flux variation in the SMA 1.3\,mm light
curve during the flares visible in May 2009, August 2010 and September
2011, coupled with the hardening in the {\it Fermi } flux at these times,
strongly suggests that whilst the energy of the electrons in the jet
increases and inverse Compton scattering is enhanced during the
flaring periods, the overall electron number density (and hence the
synchrotron emission) is relatively unchanged. Changes in the electron
population; the photons they produce and then up-scatter, depend on
the structure of the emission region. Therefore, variations at one
frequency do not necessarily lead to similar variations elsewhere in
the spectrum.

\citet{zacharias13} demonstrate the time-dependent changes seen in the
overall SED of a source during and after a flare. There is a
significant lag in the X-ray and sub-mm regimes to a flare in the
$\gamma$~rays and optical of days to weeks.  This matches the observation
that NGC\,1275 exhibits enhanced TeV emission in periods of flaring
\citep{aleksic12,aleksic13}. The \citet{zacharias13} models suggest
emission in the optical and $\gamma$~rays will show a more direct link in
their variability. The simultaneous study of $\gamma$-ray and optical
variability has only been possible since the launch of {\it Fermi } and
\citet{aleksic13} present the first attempt to investigate this: the
flux of the two datasets are well correlated. They use optical data
from the KVA\footnote{http://users.utu.fi/kani/1m/} optical
monitoring, covering the past four years, which confirms that the
short-timescale ($<$month) variation in optical flux visible in the
\citet{lyutyi77} and \citet{nesterov95} results has returned.

Given the rich variety in the variability and relative brightness of
NGC\,1275, it is to be hoped that it will continue to be monitored at
all wavelengths (especially in the optical and TeV), and more
frequently over the next few years of increasing activity, to search
for direct temporal correlation between the mm/sub-mm, near-infrared,
optical and $\gamma$-ray emission.

\subsection[]{Wider implications}
\label{ssec:implications}

The variable nature of NGC\,1275 has implications for our
understanding of other BCGs in cooling-core clusters. It is known that
the X-ray emission from BCGs is variable \citep[e.g.][]{russell13} and
that a substantial number of GHz-peaked sources are found in BCGs,
both with and without additional, steeper-spectrum components (Hogan
et al., in preparation), but as yet there have been no systematic
searches for radio variability in BCGs in the literature. The example
of NGC\,1275 is an important one, as it highlights the fact that
relying on data from below 10\,GHz can overlook the contribution from
a synchrotron self-absorbed core.

This is particularly important when considering the contamination of
Sunyaev-Zel'dovich (SZ) effect observations in the 30--150\,GHz range,
where the measured decrement could be underestimated if the additional
high-frequency, point source component is not accounted for \citep[see
  e.g.][]{knox04,coble07,lin09}. For instance, the 1.4\,GHz flux
density for NGC\,1275 is comparable to the 100\,GHz {\it Planck} flux
density at $\sim$10--12\,Jy in 2010 but an extrapolation from the
steeper-spectrum emission at lower frequencies would predict a flux of
$\sim$\,0.1\,Jy.  Using NGC\,1275 as an example of such a
contaminating source, it is clear that having radio data over a broad
frequency range and within a few years of the SZ observations is
essential to correctly account for this variable, flat-spectrum core
emission.

We can also use the observed ratio of radio to $\gamma$-ray emission in
NGC\,1275 to estimate the possible {\it Fermi } fluxes of other
BCGs. Scaling from the 2010 fluxes at 90\,GHz and between
0.3--300\,GeV of 10\,Jy and 3$\times 10^{-8}$ph\,cm$^{-2}$\,s$^{-1}$,
respectively, the next brightest BCG in the radio band would be
50--100 times fainter in the $\gamma$~rays, so undetectable at the current
{\it Fermi } exposure level. This agrees with the analysis of
\citet{dutson13} who considered a sample of 114 core-dominated BCGs
and found no individual {\it Fermi } detections apart from two AGN-dominated
sources, already established as HE emitters. Nor was a signal found by
co-adding the BCG candidates, so it is uncertain whether it is the
proximity of NGC\,1275 that makes it exceptional, or that it is in
itself peculiar. Its current state is not necessarily typical of the
source; continued monitoring decades into the future might address
this uncertainty, establishing observationally a complete cycle into
and out of an active state. If another moderately bright BCG were to
experience an outburst, then {\it Fermi } ought to be capable of detecting
it (particularly during flaring events) but it would require long-term
monitoring of dozens of systems at $>$30\,GHz to identify possible
candidates.

The properties of NGC\,1275 can also inform our understanding of radio
galaxies and BL\,Lac objects. The beaming of the core that makes
BL\,Lacs so prominent also acts to shorten the observed variability
timescales at all wavelengths, by an order of magnitude in many
cases. Therefore, the outburst timescale observed in NGC\,1275 of a
few decades with at most {\it mild} beaming \citep{nagai10}, is
comparable to the few-year outburst timescale seen in sources such as
3C\,279 and 3C\,454.3, where the beaming is a factor of order ten
higher. Thus, when considering the core dominance of radio galaxies it
is important to take into account both the self-absorption of the
core, and its potential variability on decade-to-century
timescales. The observed properties of NGC\,1275 show very little
variation below 1\,GHz, so selecting a sample of radio galaxies at low
frequency (e.g. 159\,MHz using the 3C Catalogue; \citealp{edge59})
would select sources like NGC\,1275 uniformly, as the level of core
activity has little or no effect. However, making the selection at
$>15$\,GHz (e.g. The Australia Telescope 20\,GHz Survey; AT20G;
\citealp{murphy10}) would depend greatly on when in the last 50 years
the object was observed. Ensuring that the `time domain' aspects of
the properties of radio galaxies are considered will help build a more
self-consistent picture of both beamed and non-beamed radio sources,
and the emission mechanisms that give rise to their extraordinary
multiwavelength properties.

\section[]{Concluding Remarks}
\label{sec:conclusion}

NGC\,1275 has been pivotal to our understanding of AGN feedback over
the past three decades \citep[see e.g.][]{bohringer93,fabian00}. The
presence of multiple `bubbles' in the intracluster medium of the
surrounding cluster indicates that there are major outbursts from the
core on timescales of 10$^{6-7}$\,years.

Building on previous work, this paper provides striking evidence for
variability of NGC\,1275 on decade timescales, showing that there are
repeated outbursts from the central few parsecs of the source, which
vary in amplitude by about an order of magnitude.  On top of this
episodic variability there is also short-timescale flaring activity
seen over a few days to a month in the $\gamma$~rays, that can produce an
additional order-of-magnitude brightening in flux and coincide with a
detection at TeV energies.

NGC\,1275 is currently brightening rapidly and may reach a luminosity
similar to that observed for over a decade in the 1960's and
1970's. The much broader range of multi-wavelength facilities
available now will present an unprecedented opportunity to study the
behaviour of the source during a very active phase. In particular,
linking the shorter-timescale $\gamma$-ray variability to the launching of
individual radio components in the jet \citep[e.g.][]{suzuki12} is now
possible with continued monitoring with long baseline interferometers
at high frequency ($>$20\,GHz). Therefore, the current outburst will
provide us with an opportunity to witness processes at the very heart
of AGN feedback.

\section*{Acknowledgements}

The SMA is a joint project between the Smithsonian Astrophysical
Observatory and the Academia Sinica Institute of Astronomy and
Astrophysics, and is funded by the Smithsonian Institution and the
Academia Sinica. This work has made use of public {\it Fermi } data and
Science Tools provided by the {\it Fermi } Science Support Centre, the
NASA/IPAC Extragalactic Database (NED) which is operated by the Jet
Propulsion Laboratory, California Institute of Technology, under
contract with NASA, and the SIMBAD and VIZIER databases, operated at
CDS, Strasbourg, France. We thank Margo Aller for permission to use
data from the University of Michigan Radio Astronomy Observatory,
which was supported by the National Science Foundation and NASA, and
by funds from the University of Michigan. We thank also Richard White,
whose automated {\it Fermi } tool chain improved the time-efficiency of much
of the analysis carried out. K.~L. Dutson acknowledges support from
the STFC studentship ST/I505780/1 and the STFC Doctrinal Training
Grant ST/J501104/1, M.~T. Hogan from the STFC studentship
ST/I505656/1, W.~N. Alston from the EU FP7-SPACE research project,
STRONGGRAVITY., J.~A. Hinton from the Leverhulme Trust, and A.~C. Edge
from STFC grant ST/I001573/1.

redpajama_set_name: RedPajamaArXiv


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Matt & Kerin's beach-side Falmouth Wedding was certainly no exception!
The day was just perfection, from start to finish!
& a whole lotta dancing!
Matt & Kerin, thank you so much for allowing me to be a part of such a special day in your lives!
I recently had the pleasure of getting to hang out at the beach with the Galligan family.
It's been about 3 years since the last time we got together for some pictures, so I was more than happy to be able to get together again and see how much the kids have grown!
And boy had they grown!
We moved along the beach pretty quickly, trying to keep each pose more like a 'new adventure' for little sister.
I couldn't have done it without big brother and sister to help me out every step of the way!
One "adventure" was, well, maybe not completely thought out…. and may have fallen apart in slow motion….
You see it, i know you do…. step, step….SPLAT!
What's a little mud between family?! Right?
…and when all was said and done, everyone was still smiling!
I recently had the pleasure of getting together with Joshua for his senior session.
I actually remember the day Joshua was born, and have had the pleasure to watch him grow into the amazing young man he is today.
We had a lot of laughs, walking through Ellisville State Park and looking for little nooks and areas to photograph in.
These were some well groomed poison oak trees!
All in all, it was just a great time, hanging out and being goofy….
Definitely another great memory made.
Of course, I wouldn't being doing my job as his big sister if I didn't add a funny little blooper.
I'll spare you all, and just choose one of the many!


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5. Be reliable: The easiest way to get off to a good start is to do your work on time and to do it well. When your co-workers and boss are confident with your work you're less likely to run into any job related performance issues.
6. Keep your boss informed: Hold regular meetings with your boss during which you can give him or her a status update on the major projects you're working on, and provide a forum to ask for any help or guidance you need. This will help ensure that you're on the right track, and can provide a regular way to show your boss that you're doing great work.
7. Make time for meetings: Make sure to take time out of your schedules for non-mandatory professional meetings. Joining an optional working group, enhancing your skills through training or just getting exposure to people you normally wouldn't work with are all great ways to network within your organization and can help you gain important skills and responsibility.
8. Be flexible and open-minded: Remember that there are often several ways to solve a problem or achieve an objective. Do not insist that your idea or plan is always the best one. By remaining open to advice from others, and to new ideas, you'll be able to look at solving problems from a new perspective, which is key to anyone's growth.
9. Gain the confidence of others: Give credit to others when they do a good job, and simply reply with 'thank you' when others do the same with you. Your co-workers will appreciate the credit you give them, along with your lack of arrogance. Another great way to gain confidence is by looking credible in face to face interactions through proper body language and active listening.


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My life and times, simplified into a blog. Fire away!
The Official Carlos Alomar Blog
A Letter From The Editor
Carlos Alomar
Big Boys Timeline
Touring With The Big Boys
THE BIG BOYS
Alicia Keys – 2009
Mick Jagger-1985
Rap-Hen-G and Evil-E
Carly Simon – 1994
Peter, Paul and Mary
Belouis Some – 1985
Jimmi Destri
Arcadia-1985
Sesame Street – 1970
Taramasa Hino
International Acts
Casiopea
Alberto Fortis
Fabiana Cantillo
After 32 International gold and platinum records, Carlos Alomar's place in music history is secure. The legendary guitarist burst upon the rock scene with David Bowie in the mid-1970s, when he, Bowie, and John Lennon co-wrote the hit song "Fame." Over the course of the next 30 years, Alomar would record and tour the world as Bowie's music director. His ability to play R&B, Philly soul, hard rock, and ambient music meant that he was always in demand – and able to keep up with Bowie's quicksilver changes of musical persona. He also co-wrote Mick Jagger's first solo effort, "She's The Boss," Iggy Pop's comeback hit "Sister Midnight," and played guitar for a Who's Who of pop/rock royalty – from Paul McCartney to Simple Minds.
As a rare Latino musician in the rock scene, Alomar also occupies a singular place in Latin music history. Over the years, as a producer, co-founder of the National Rock Movement of Puerto Rico, and advisor to the Latin Academy of Recording Arts and Sciences (LARAS, the organization that does the Latin Grammy Awards), he has championed Latino rock musicians.
But Carlos Alomar is not about history; he's about the future. While remaining active on the music scene, working with contemporary artists like the Scissor Sisters and Alicia Keys, Alomar has also become a cutting-edge figure in the worlds of music education and music technology. Now, as the Distinguished Artist in Residence at Stevens Institute of Technology, Alomar is pioneering the use of digital technology as a means of giving young musicians the tools to change the way music is made. And he's doing it at a university that is uniquely positioned to allow its students to do just that: Stevens has a 140-year tradition of combining academics, research, and hands-on, real-world experience in the fields of science, engineering, and entrepreneurship, earning its reputation branding as "The Innovation University." read more…
Robin Clark is an American vocalist best known for her work with the UK band-Simple Minds on their "Once Upon a Time" album and tour. Robin has a rich history of working in all fields of the entertainment industry; recording studios; national and international commercials; T. V.; radio;touring and on Broadway.
Robin Clark's life has been more than a "Dream Come True". A native New Yorker who grew up in a home filled with music and entertainment. In 1984 Robin was discovered by John Hammond, who released her solo album "Surrender" with songs written by some of the most prestigious songwriters in the business as well as featuring David Bowie's Band.
Robin has appeared in the major motion picture "Keeping The Faith"
Starring Ben Stiller, Jenna Elfman and Ed Norton as well as providing vocals on Sound tracks for Disney films "Tarzan", "Aladdin "and the FOX film "Anastasia". Robin has also performed for the Broadway productions of "The Wiz" and "Got To Go Disco".
Her Television appearances include: Sesame Street, The Conan O'Brian Show, Saturday Night Live, David Letterman, Jay Leno, Ellen DeGeneras Show, Vanessa Williams' "Home For Christmas" special, Good Morning America, The Today Show, The Oprah Winfrey Show and "Looking For Elvis" a T.V. Special.
Robin has received numerous Gold and Platinum CDs for her contribution to the music industry. She has had the good fortune to work for some of the music industries most well respected and award-winning producers. She has sung for some of the premier artist of our times including Michael Jackson, Britney Spears, Mary J. Blige, Bette Midler, Michael Bolton, Ringo Starr, Shania Twain, Bob Dylan, Leona Lewis, Simple Minds, Chic, Scissor Sisters, , Teddy Pendegrass, Natalie Cole, George Benson, Al Green, Tina Turner, The Blues Travelers, Spin Doctors, Blur, Barry White, Frankie Valli, Moby, Dolly Parton and Aretha Franklin…just to name a few.
Here are some additional examples of her accomplishments:
11 Albums with Luther Vandross,
A Performance on the Queen Mary II w/ Beyonce,
A 9/11 Tribute "For Hero's Sake" W/ Sheryl Crow,
Performing for "The Grammy Honors Mariah Carey and Jay-Z",
Singing with Jill Scott, Moby and The Blue Man Group for the Grammy Awards.
She has also Toured and recorded with David Bowie, Laura Nyro, Patti Scialfa and Bruce Springsteen. Internationally she had toured and recorded with Japanese supergroups "Dreams Come True" & "Funk the Peanuts"
But…. history is still being made. Currently she is the voice of the "Orange Bear clock" for the award-winning Nickelodeon television show 'Team Umizumi" as well as recording with Glee's-Matthew Morrison.