Digital review is a place where infographic style meets the current trends. While traditionally formal assessments are considered to be boring and insipid; however, when it comes to website design sphere, everything takes a whole new look.
With different dynamic effects and a bunch of instruments for prettifying interfaces, the statistics-related projects are just destined to look fantastic, prominent and exceptional. Artists get rid of formal and serious interfaces and adopt original and entertaining solutions that shed the light on numbers in a delightful fashion, transforming an overview of past year into an exciting adventure.
Animations, illustrations, videos, typography, icons and other elements are involved in this metamorphosis. Our today's collection includes namely such concepts. They are juicy, original and trendy.
Explore the list and tell us, which is your favorite?
This year the portal is the 'talk of the town'. It is a real trendsetter. It comprises not one but a range of outstanding photos made in a chic duotone technique.
Dynamic behavior and layering aesthetics are other factors that give the project a cutting-edge look.
The agency opts for a clean and minimalistic design that is packed with fresh air, flat graphics and fancy animations. A rough geometric typeface that marks the 'welcome' section is the only thing that adds to a businesslike atmosphere. The rest of the design is playful and amusing.
The review is defined by a modernized take on a classic layout with a plenty of whitespace. The grid is used to demonstrate key points and special effects to draw the attention. Splashes of bright purplish gradient, outstanding authentic techno typeface, halftone style animations: the page is pretty original.
The team bets on a traditional display of data, getting the most out of common infographic-related elements such as charts, maps or diagrams. These graphical representations are skillfully bolstered by subtle motion that add dynamics and enhance the visual experience.
Year in Review by Behance is rich in lavish images that reveal interesting stories. It is bold, eye-catching and at the same time informative.
The page is a combination of gorgeous gradients and sumptuous shots.
The news portal follows the philosophy of ' A picture is worth a thousand of words'. The recap demonstrates the great stories of the previous year in a visual manner, choosing images instead of text. Each one is supplied with a tiny description.
The Goliath of the industry stays true to itself by offering visitors a video review. The latter lasts just seven minutes, yet it is amusing and engaging and perfectly reflects the spirit of the platform.
Tumblr's Year in Review has a bit nostalgic aura because of outrageous coloring, abstract animations and poster style blocks.
The page evokes the feeling of a slight mess, yet the grid structure saves the day. It lets users scan the top posts, top memes, and other stuff without hassle.
Year in Review by Vox Media has an artistic nature. Brilliant vector illustrations that are made in a soft pastel color scheme reinforce the theme and create the overall aesthetics. The collection of highlights is dished up to the targeted audience in an enjoyable way.
Year in Review by Pingdom matches the tone of the online service. It looks innovative and high-end. Techno vibe is prevalent. Guided by the visual path the users naturally flow through the content stream, familiarizing themselves with numbers.
The review is created on a top of a conventional horizontal stripe layout. There is nothing unusual. However, everything looks intriguing and engaging.
The team focuses on revealing only favorite stories and vital data using lots of complementary graphical material. Their illustrative approach will certainly make you smile.
The team offers their fans to indulge once more in reading the best articles and tutorials created by the community. While the collection includes only innovative and the most popular write-ups, the design with its beautiful saturated gradient and lovely typography meets modern trends, bolstering the portal's brand identity.
The company invites visitors to enjoy a recap of the previous year, which was quite productive and profitable. The review speaks completely through numbers that are supported by a fancy environment. The team employs images, abstract backgrounds, dynamic elements and animations to skillfully dish up the content.
This multimedia-centric design will easily draw you into thanks to a bunch of incredible pictures. Although the project is overpopulated with visuals, yet the design remains clean and fresh.
The website offers a brief examination of the highlights of 2015.
The team plays heavily on an illustrative approach and subtle effects, creating a splendid composition. It is rich in key moments that are presented in a relatively formal manner. The page maintains the user's focus all the time, gently prompting to scroll down.
The beauty of the project lies in a wise combination of graphics, text and typography. These three factors create the whole aesthetics and place priorities. The page does not have any clear boundaries so that the content flow is flowing and continuous. Thanks to copious amount of whitespace it does not overwhelm readers.
Although the environment is visually stimulating, however the numbers always stay in focus.
The team has skillfully set the stage for the content by utilizing a traditional linear layout. However, it is the only thing that is boring. Harmonious and soft duotone effect steals the show here. It delivers the right feel for the project, injects some energy and gives the design a stylish look.
All the highlights are placed upon the solid monochrome stripes so that they easily catch the eye.
Much like Campaign Monitor's review benefits from the adaptation of a classic way of data representation. You will find in here stacked bar chart, bubble chart, colorful pie chart, and some other. Every vital detail is set in motion and activated by the parallax.
Immersive Garden has an entirely interactive overview of the past year. It is exceptional, whether you scan project through a PC or touch screen device. It unobtrusively stirs users into action.
Modern reviews mirror the trends. The majority of the listed above leverages saturated gradients, line style graphics and flat illustrations. Multimedia also plays an important role. As a result, you can enjoy boring statistics that has been skillfully encapsulated into a stylish, hip, and juicy environment.


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In the community: therapeutic yoga comes to the East Windsor Senior Center
In May, Marzena Bard, PTA, CYT presented "Yoga in Physical Therapy for Women's and Men's Health" at the East Windsor Senior Center and led participants through gentle yoga poses that can be used in rehabilitation.
vincent's story: pain with sitting
Written by Becca Ironside, PT
Vincent found our clinic by chance. He scoured the Internet, looking for a reason to explain the confounding pain in his pelvis. Vincent had a high-stress, corporate job wherein he sat all day long. He began to notice pain in his perineum while sitting. The longer he sat, the worse the pain became.
There were other symptoms, and they were even more troubling. Vincent began to have difficulty urinating. He would have the intense urge to void his bladder, but upon rushing to the bathroom, nothing would come out. Then there was the constipation. Days would go by, with no bowel movements. The discomfort and bloating in Vincent's stomach made eating food feel like he was a beaver actively working to dam up the river of his intestines. So, he stopped eating for a few days. But that did not help and the constipation persisted.
The final symptom which prompted Vincent to become desperate for help was testicular and penile pain during arousal. Vincent could no longer have intercourse with his wife without searing pain. He called a urologist and a gastroenterologist. He scheduled appointments for both specialists around his busy schedule.
The urologist prescribed a pharmaceutical named Flomax to improve Vincent's ease in urination. The gastroenterologist recommended Miralax, a bowel aide which allows water to be retained in the stool, thereby promoting softer stool and more frequent bowel movements. Both of these agents helped Vincent with about one-third of his overall complaints; but he was still unable to sit at his desk without pain, and his sex life had taken a turn for the worse. Vincent's wife was unhappy, though not as unhappy as Vincent. There has to be something out there to help me, he wondered. But what?
This was when Vincent initiated his full-throttle search on the Internet. He looked for stories of men with similar complaints. Vincent lives in Central New Jersey. There came a day when he found Connect PT online. The office was merely 14 miles from his home! He booked an appointment for the following week and crossed his fingers as he paced around his office, trying to stop the throbbing in his pelvis by willpower alone.
Upon his initial Pelvic Floor physical therapy evaluation, Vincent told his entire history to his evaluating therapist. She sat and nodded, and then proceeded to ask him a series of questions about his symptoms. To every one of the questions, Vincent longed to shout: YES! I have trouble maintaining a urinary stream! I have severe constipation! I cannot sit without pain! I cannot have sex anymore, because the discomfort is not worth the release!
The PT gave Vincent some relaxation exercises, a home program to stretch his own pelvic floor and even a link to a seat cushion which Vincent could use to take the pressure off of his perineum, rectum and tailbone. This would allow him to sit for longer periods of time with less pain, the PT said. Within a few months, Vincent was able to urinate more freely, have more consistent bowel movements, and was able to return to having sex with his wife.
How had all of this happened? Was it magic? No. But it seemed that way to Vincent. Vincent's recovery had everything to do with his willingness to seek treatment and the newfound availability of Pelvic Floor physical therapy. His symptoms were far more common than he knew. Now, Vincent writes blogs about pelvic pain in order to share his experience with other men who may be suffering from similar complaints.
The greatest outcome of Vincent's recovery was his decision to retire from his high-stress, corporate job. He still uses the special seat cushion which takes pressure off of his pelvic floor to drive across the country in an RV. Vincent and his wife have seen Yellowstone National Park, and they even take their English bulldog named Lola along for the ride. In sum, everyone is happier. Vincent, his wife and Lola. All because of one fortuitous Internet search and the prevalence of Pelvic Floor physical therapy.
"Looking back, I see that my symptoms really began to change when I began talking about this," Vincent says. "Giving a voice to the pain, isolation and embarrassment has changed everything. I just want more people to know that they are not alone."

redpajama_set_name: RedPajamaCommonCrawl


text:
Henry "Enrique" Tarrio ( , ; born ) is an American activist, former FBI informant, and convicted felon who serves as chairman of the Proud Boys, a far-right, neo-fascist, and exclusively male organization that promotes and engages in political violence in the United States. Tarrio was indicted in June 2022 on seditious conspiracy charges, along with four other Proud Boy leaders, for his alleged role in the 2021 United States Capitol attack.

Tarrio, who is of Afro-Cuban background, served as the Florida state director of the grassroots organization Latinos for Trump. In 2020, Tarrio was a candidate in the Republican primary election for Florida's 27th congressional district, but withdrew. According to a former federal prosecutor and the transcripts of a 2014 federal court proceeding, Tarrio had previously served as an informant to both federal and local law enforcement.

Proud Boys

Tarrio volunteered at a Miami event for far-right commentator Milo Yiannopoulos in May 2017 when he encountered a member of the Proud Boys, who encouraged him to join the organization. In August 2017, Tarrio attended the Unite the Right rally in Charlottesville, Virginia. He said he was there to protest the removal of Confederate monuments and memorials.

In 2018, Tarrio became a fourth-degree member of the Proud Boys, a distinction reserved for those who get into a physical altercation "for the cause"; he punched a person who was believed to be aligned with antifa. He assumed the role of chairman for the organization on November 29, 2018, succeeding Jason Lee Van Dyke, who held the position for two days, and Van Dyke's predecessor Gavin McInnes. McInnes involved Tarrio as a prospective electoral candidate, and in that capacity both conferred with Trump right-wing confidants Steve Bannon (whom Trump later pardoned) and Sebastian Gorka.

Tarrio helped organize the End Domestic Terrorism rally held in Portland, Oregon, on August 17, 2019. The event, co-organized by Joe Biggs, was framed as a response to the June 2019 assault on conservative blogger Andy Ngo.

Tarrio attended a pro-Trump march on December 12, 2020, in Washington, D.C., along with around two hundred other Proud Boys. He was arrested in connection with the march on a misdemeanor destruction of property charge related to the burning of a Black Lives Matter banner stolen from a church. In August 2021 he was sentenced to five months in jail for the incident and on a weapons charge.

In January 2021, Reuters reported that Tarrio had been an informant to both federal and local law enforcement between 2012 and 2014. This report contributed to rifts within the Proud Boys. In the aftermath of the 2021 United States Capitol attack, chapters of the organization split with the national group. Several chapters across three states pointed to Tarrio's past as an informant as a reason for their splintering from the national organization. The Oklahoma chapter also split from the national group because of Tarrio, blaming his "failure to take disciplinary measures [which] have jeopardized our brothers' safety and the integrity of our brotherhood". Tarrio himself did not participate in the attack, having been arrested two days earlier in Washington, D.C., and ordered to stay away from the city. Later, he said he would neither "support" nor "condemn" the attack and did not "sympathize" with lawmakers.

Career
After 2004, Tarrio relocated to a small town in North Florida to run a poultry farm. He later returned to Miami. He has also founded a security equipment installation firm and another providing GPS tracking for companies. Tarrio owns a Miami T-shirt business, known as the 1776 Shop, an online vendor for right-wing merchandise. Slate described the 1776 Shop as a "freewheeling online emporium for far-right merch" that sells a range of Proud Boys gear including shirts stating "Pinochet did nothing wrong".

Political views
In regard to his views on extremist groups and ideologies, Tarrio has been quoted as saying, "I denounce white supremacy. I denounce anti-Semitism. I denounce racism. I denounce fascism. I denounce communism and any other -ism that is prejudiced towards people because of their race, religion, culture, tone of skin." In regard to his own ethnicity, he has said, "I'm pretty brown, I'm Cuban. There's nothing white supremacist about me."

After Tarrio confronted and shouted expletives at House Speaker Nancy Pelosi in Coral Gables in late 2018, the chairman of the Miami-Dade Republican Party apologized and U.S. Senator Marco Rubio compared the disruptors to the "repudiation mobs Castro has long ago used in Cuba."

In 2018, Twitter removed Tarrio's account, along with others related to the Proud Boys, citing how platform policy prohibited accounts related to violent extremist groups. The following year, Twitter detected and removed another account that Tarrio created to evade the suspension.

Tarrio said he is a close friend of Roger Stone, a Trump ally who is a high-profile Proud Boys supporter. After Stone was arrested in January 2019, Tarrio appeared outside the courtroom in a shirt emblazoned with the message "Roger Stone did nothing wrong". The two appeared in a video together made on December 11, 2020, the day before a "Stop the Steal" rally where Tarrio stood on stage with Stone. On December 23, 2020, Trump pardoned Stone, whose prison sentence he had previously commuted.

Tarrio began a run for Congress for Florida's 27th district in 2020, but withdrew before the Republican Party primary. In his campaign's responses to a Ballotpedia survey done in 2019, Tarrio listed criminal justice reform, protection of the Second Amendment, countering domestic terrorism, ending the war on drugs, free speech on digital platforms, and immigration reform among his priorities.

Arrests
In 2004, when he was 20 years old, Tarrio was convicted of theft. He was sentenced to community service and three years of probation and was ordered to pay restitution.

In 2013, Tarrio was sentenced to 30 months (of which he served 16) in federal prison for rebranding and reselling stolen diabetes test strips.

According to a January 2021 Reuters report, between 2012 and 2014 Tarrio had been an informant to both federal and local law enforcement; in a 2014 federal court hearing, Tarrio's lawyer said that Tarrio had been a "prolific" cooperator who had assisted the government in the investigation and prosecution of more than twelve people in cases involving anabolic steroids, gambling, and human smuggling; had helped identify three "grow houses" where marijuana was cultivated; and had repeatedly worked undercover to aid in investigations. Tarrio denied working undercover or cooperating with prosecutions, but the court transcript contradicted the denial, and the former federal prosecutor in the proceeding against Tarrio confirmed that he cooperated.

On January 4, 2021, Tarrio was arrested by Washington, D.C. police and charged with one misdemeanor count of destruction of property in connection with the burning of a Black Lives Matter banner stolen from a Washington, D.C. church during a pro-Trump march on December 12, 2020, that drew around 200 Proud Boys. Tarrio acknowledged that he had burned the banner, but denied that the act was a hate crime. A statement released by African Methodist Episcopal Church, which was one of two historically Black churches in D.C. targeted on December 12, said that the church had sued Tarrio and the Proud Boys organization. Tarrio was also charged with two felony counts of possession of a high capacity feeding device after two high-capacity firearms magazines were found on Tarrio when he was arrested. His request to be allowed to have Bevelyn Beatty, a Black Christian activist who was herself accused of defacing a Black Lives Matter mural, to testify for him as a character witness was summarily denied. As a condition of his release on bail on January 5, 2021, Tarrio was banned from entering Washington except for trial or meeting with his lawyers.

January 6 United States Capitol attack
The FBI later said they had arrested Tarrio in an attempt to prevent the 2021 United States Capitol attack.
On July 19, 2021, Tarrio pleaded guilty to a destruction of property charge and a reduced charge of attempting to possess a high-capacity ammunition feeding device.

On August 23, 2021, Tarrio received a 155-day prison sentence, more than the 90 days requested by Department of Justice prosecutors. Tarrio began serving his sentence on September 6, 2021. His November 2021 request for early release based on poor living conditions in the D.C. Jail was denied.

By November 2021, at least two dozen Proud Boys members and affiliates had been indicted for their alleged roles in the 2021 United States Capitol attack. Tarrio and the Proud Boys were subpoenaed by the House Select Committee on the January 6 Attack in November 2021 relating to the organization's alleged involvement.

In March 2022, Tarrio was indicted on a conspiracy charge by the Justice Department for his involvement in organizing the January 6 attack. On June 6, 2022, the Justice Department announced that Tarrio and four other members had been indicted on more serious seditious conspiracy charges.

On December 19, 2022, the trial of Tarrio and four co-defendants began after U.S. District Judge Timothy Kelly denied defense attorneys' last-minute bid to delay jury selection. The trial has continuously been plagued by delays due to on-going disagreements between Tarrio's legal team and the Judge Kelly, including multiple requests for the case to be declared a mistrial.

Personal life
Henry Tarrio was born in  and raised Catholic in Little Havana, a neighborhood in Miami, Florida. Tarrio is of Cuban heritage and identifies as Afro-Cuban. He is divorced.

References

External links

1980s births
Living people
Activists from Florida
Candidates in the 2020 United States elections
Critics of Black Lives Matter
American people of Cuban descent
American neo-fascists
Businesspeople from Florida
Florida Republicans
People from Miami
People of Afro–Cuban descent
Police informants
Proud Boys
Year of birth unknown
People criminally charged for acts during the January 6 United States Capitol attack

redpajama_set_name: RedPajamaWikipedia


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text:
ED2011 2/5 Reviews ED2011 Theatre Reviews
David Lee Nelson… Status Update (David Lee Nelson)
By Ivan Juritz | Published on Friday 19 August 2011
A failed hybrid of theatre and stand-up comedy, 'Status Update' is a one-man monologue showing a man trying to find humour in a lonely existence after divorce. Nelson aims to steer between tragedy and farce, but fails to settle comfortably into either. The monologue is interspersed with long and tiresome home-videos in which he recounts the sour details of his marriage. There are moments of muted inventiveness, but Nelson's stand-up is too staged to strike the intimate tone he aims for. The unexplained use of pre-recorded video adds nothing to the performance. It is a show that, in its close attention to David Lee Nelson himself, would benefit from an affable quirkiness that he entirely lacks.
Laughing Horse at The Beehive Inn, 4 – 28 Aug (not 8, 15, 16, 22), 3.45pm (4.40pm), free, fpp254.
tw rating 2/5
[ij]
READ MORE ABOUT: Laughing Horse Free Festival


Open source in government. Sourcefire announces relationships with Symantec and Microsoft. EPL supercedes CPL. The cost and potential savings of open source. The origins of open source. IBM and Sun - back on? And more.
# OStatic: Why Isn't Open Source Even Considered at the U.S. State Government Level?
# Simon Phipps: Five Ideas To Get FOSS Into Governments.
# Sourcefire's 3D system to be bundled as part of the Symantec Managed Security Services offering.
# Sourcefire has also announced a strategic relationship with Microsoft.


Aire Serv is a leading national heating and cooling franchise with a primary focus on helping our franchisees meet and exceed their financial, professional and personal goals. As part of the Dwyer Group family of brands, our expertise lies in providing exactly the right tools, support and environment to turn those goals and dreams into a reality. We see it happen every day. Why shouldn't it happen to you?


I saw this at 2019 NAMM, I got one and I love it. I don't like onboard digital OD units, I prefer clean to that. But this thing is very "Organic" as you pour on the volume, it gets nasty.
It is supposed to simulate the output of the AO-28 amplifier in the hammond. I believe that is a mono device; the Tall, Fat AND WIDE outputs in stereo.
Yes, this is a mono Overdrive. The Tall and Fat, Preamp. and Boost, Tall, Fat And Wide Stereo version.


text:
2014.11.13 | 2015.01.28
VIEW ARTIST
A arte Invernizzi and Lorenzelli Arte galleries opened on Thursday 13 November 2014 two one-man exhibitions of the works by Rodolfo Aricò. The exhibition itinerary, ideated in a unitary way for the two galleries, intends to present and examine the artist's activity from the middle of the 1960s until the opening years of the 1990s by way of a choice of fundamental works.
The rooms of the A arte Invernizzi gallery housed examples of the Senza titolo series of 1967, works that evidence a reflection which questions the potentialities of formal expressive reduction. During those years and the following decade Aricò analysed and carried out research regarding the diverse structural and expressive modulations bound to primary forms, applying himself to a type of investigation that was not only spatial but also dimensional and chromatic, as can be seen in another work on exhibit entitled Arco B of 1970.
With Area/Prospettiva of 1972, exhibited in the one-man exhibition held at Palazzo Grassi in Venice in 1974, the original geometrical model became a sequence and defined a unitary work, structurally composite, on the surface of which the colour is qualified as a heterogeneous spreading that is made to vibrate thanks to light.
The 1980s, which represent a fundamental turning point in the artist's coherent and progressive career and that give rise to works such as Cenere of 1987 (also on exhibit in the A arte Invernizzi gallery), unfold in decisive openness with respect to a lyrical dimension in which life and painting create a both heterogeneous and total amalgamation. By way of images Aricò arrived at rendering the drama of human existence. The canvases of this period are structured in less geometrically defined forms with respect to the previous ones based on axonometry or projections.
The artist's cognition of vital tension as movement capable of the breakage of finite limit accentuated his need in painting to transcribe the totality of the absolute, embodying the perception of it in a sole moment: that of the event of the work. Corresponding to a variation in the shaping of the canvases, one also has a diversification with regards to the spreading of the colour which is rendered 'multiple' and irregular. During the 1990s this choice became increasingly more pronounced in his works: examples of these are exhibited both in the A arte Invernizzi gallery (such as Circumflex and Aspro of 1991, the latter characterised by a very angular and irregular structure) and in Lorenzelli Arte. In these last works which close the exhibition installation the various tonal modulations are scratched and crossed by irregular and broken lines: here one has the accentuated sensation that the colour, even if it clearly shows itself, conceals something that eludes the eye, as if the works were suspended, in balance within the description of mankind's drama.
On the occasion of the exhibition a bilingual monograph, edited by Luca Massimo Barbero, has been published with the reproductions of the works on show and an up-to-date bio-bibliographical notes.


definitely getting this. pre-orders on amazon only run about $75, which is an insane deal if you really think about it. would prefer they kept the original coloring though.
Ah... my favorite run on The Mighty Thor. Simonson was simply producing one great issue after another. Even though I have all of the original issues, I am going to get this Omnibus. It's just too cool to pass up.
I am a little confused by the covers... what does round 1 and round 2 mean?
Hey there, I think it's Simonson's odd way of referring to each of the cover versions.
Well, if get to choose... I will have to get the one with Beta Ray Bill on the cover!
I hate this computer colouring crap. Just looks like puke. Visual vomit. Gradients and flares everywhere. No tonal sensitivity whatsoever. Give me newsprint and manual colour craft over these photoshop knob jockeys any day. This is the complete ruin of a classic run. Get the original issues - it's the only honest option.


text:
DeKalb graduates thank teachers who helped them
By ANDREW KINGEmail
Photos by Mark Black for Shaw Media
DeKalb High School graduates celebrate Saturday at the Northern Illinois University Convocation Center in DeKalb.
Nigel Dyson gives the farewell address during the graduation ceremony.
DeKALB – "Shrek." Kendrick Lamar's "Humble." "The Lord of the Rings."
Those pop cultural touchstones (and several others) got shoutouts during a nostalgic commencement ceremony for DeKalb High School graduates Saturday at the Northern Illinois University Convocation Center.
Principal James Horne referenced the green ogre, the films "Monsters Inc." and "The Lord of the Rings" as the films that were dominating the box office when members of the Class of 2019 were born 18 years ago.
This past weekend, they became the first crop of high school graduates born into the post-9/11 world.
In her welcome speech, graduate Emma Carpenter referenced the rapper Kendrick Lamar's ode to humility as a reminder the Class of 2019 took to heart during their high school years.
And like the hobbits of Middle-earth, these graduating seniors had a supportive community that encouraging them to keep going.
"My parents were always there for me, my friends had my back, but I have to give [credit] mostly to Mr. [Chad] Gregory, my art teacher," said Asher Lowrey, who will be attending the Milwaukee Institute of Art and Design in the fall. "This year was my last time at the DeKalb Art Show, but I've been participating in it nine years. Last year, I was considering dropping out and just pursuing the arts as an individual.
"And Mr. Gregory was the one who convinced me to come back one more year, at least for a semester, and he told me that if I came back he would find me a college I wanted to go to. And now I'm here, with $72,000 to the school of my dreams. So he pulled through, and I just had to have a little faith in him."
Christian Ibarra, who will be attending the University of Illinois to pursue a degree in business, also thanked teachers for their help on his journey, giving credit to educators Nate Viland, Tait Hilmer and Rebecca Powers.
But most importantly, he thanked his mom, Sylvia.
"She's No. 1," he said. "She's my best friend."
At graduation, many turned their attention to another champion of DHS students who was unable to attend the ceremony. Brenda Shakir commemorated her late husband, Ata, who passed away in June 2017 after a four-month-long battle with cancer.
Ata Shakir was a social studies teacher at DeKalb High who was 41 when he died.
"He didn't want you to impress him," Brenda Shakir said. "He wanted you to impress yourself."
Senior class president Nigel Dyson said Ata Shakir inspired him during his years at the high school.
"I think the person who made the biggest impact on me was Mr. Shakir," Dyson said. "It's sad to say that he couldn't be here today because he loved graduation. But he was my first teacher in summer school of ninth grade, and you could just tell from the get-go that he believed in his students."
"Let's Dance" Big Bang Weekend waltzing into 14th year
order detention vigil set for Friday
To avoid more stalemates, DeKalb Park District board seeks 5th member
DeKalb organizers to celebrate Pride Month with community party
DeKalb Fire Department receives $3,000 grant


Born in Southern Germany, Philipp Crass grew up in a rural area immersed into nature. This early period of his life influenced the Berlin-based designer's creative approach. All of his projects showcase a strong bond to nature, but Organico may be one of most evocative examples of Phillipp Crass' work. Using both traditional and renewable resources, the designer developed a new technique to create an innovative material. Made with a blend of hemp fibers and an adhesive that combines calcium hydroxide and casein, the material is tough as well as flexible.
The "sandwich-like" structure of the material ensures its durability and strength while allowing it to easily adapt to different shapes. The Organico series presents the possibilities of this sustainable technique. The chairs feature a wooden frame which supports the eco-friendly hemp-based material. Colors and textures enhance the designs further. A blend of modern design and organic features, the concept proposes an ingenious way to craft green furniture for contemporary living spaces. Photographs© Philipp Crass.
Concrete bathroom accessories for minimalism lovers. Keeping a bathroom looking minimal and airy is easy….


AVANTech (Columbia, SC) acquired Mid Columbia Engineering (Richland, WA).
Halff Associates (Richardson, TX) acquired Genesis and its construction engineering & inspection company, Genesis CE&I Services (Tampa, FL).
Zuendt Engineering (Greenville, SC) acquired Johnson-Frey-Turzak Group (New Port Richey, FL).
GEI Consultants (Woburn, MA) acquired Savanta (St. Catharines, Canada).
BDP (Manchester, UK) made a strategic investment in Quadrangle (Toronto, Canada).
CET UK (Derby, UK) acquired Enverity (Newark, UK).


Here is a sample of the explosive second issue of mine and new series. In this issue Bunny's younger brother and sister have been kidnapped, and Bunny and Foxy must rescue them. This whole series is like an 80s action movie, big muscles, big action, big explosions, and just a whole lot of fun. There are feats of strength as Bunny does a superman/muscle hoodini chain-break escape, and Foxy does Samson pillar smash to bring down the HOUSE! And I top it all off with a dash of female muscle growth to just make things a bit better, as FMG always makes everything better!
The comic can be purchased at my shopify page my site Mighty Female Muscle Comix Shopify or via my membership site Mighty Female Muscle Comix Membership.


One surprise came after another. First my brother arrived together with one of my high school colleague and friend to say good bue in person. Then his wife Edit and his son Bence arrived. The were still there when Miklos and his girlfriend arrived. hey handed the door handle to each other. It was very emotional. Most of us were fighting against crying out loud. My wife just could not handle it so she cried. Which was understandable and OK. In the main time I received a message from Kiss Dénes the member of the Tenere Club in Szeged. He asked me if he could join me until Sabadka. I was very happy. I met him on he road and we had a drink together talked a little bit and headed towards Sabadka. Here we said our good byes and I continued to Backa Topola. In Topola Joci and Ado was waiting for me. It happened that Joci was celebrating his birthday and invited his friend. Most of them I knew from before. He had a held pig roasted. The table was full of food and drink. We had an excellent evening.


The OP is clearly a misogynist who equates treating women fairly and decently with an assault on his distorted and enfeebled masculinity.
Not wanting to be insulted and a leap to misogyny and the other things is a big one.
I personally don't have an issue with the advert, and the bulk of it is showing men behaving in a good way.
The first part, showing men behaving badly isn't nice, and it will be construed by some as a general attack, although, I believe it's filmed in a style of 'this is how things used to be' .
So, congratulations to the OP and anyone else who boycotts Gillette's products, the animals thank you.
I've just seen the advert and although it is a bit clunky it is making a fair point! I do love these snowflake men who see feminist conspiracies everywhere.
I am aware of the OP's intentions, I just think his head must be spinning if he thinks he's now supporting a boycott by tree huggers.
Isn't the bulk of the ad showing men doing the right thing? Breaking up a fight , stopping somebody jumping in on a woman.
It missed the part when the man stopping a fight was stabbed and beaten to death by the rest of the yobs.
I've no problem with the ad or the message, just the cynical way Gilette are using it to sell their products.
Boycotted them years ago when I bought a Braun electric razor.
About the same as me then. A lot easier.
It's as cynical as Sainsbury's using the 1914 Christmas truce as a way to sell more groceries at Christmas, but at the bottom of it, all advertising is similarly cynical and self serving.
This is just a company realising that their 'butch' advertising is way out of line with current thinking and failing to do better with their next attempt to convince people that they have an ethos other than 'buy our products'.
I wonder how many on here feel that is a very much a misandrist reply.
I think most men today have boycotted razors for a very long time.
I'm sure you're aware of the hoo-hah over an advert for Gillette razors, so I won't link to it, which is loaded with feminine poison about how terrible males are. Insulting your primary market isn't a very smart move.
Men everywhere should now boycott Gillette products.
see the right wing snowflakes have something else to be offended by dont you get ill with the continuous rise in blood pressure from all this anger?
I do hope that all the individual actors/extras that are on screen in the advert are ridiculed and sent to Coventry, so to speak, in their individual personal lives.
What are you smoking, dude?
I admire your balls for coming back for more ridicule.


text:
Samsung Has Acquired MOVL To Build Out Better Multiscreen Mobile And TV Apps
Ryan Lawler	@ryanlawler / 8 years
Over the last few years, Samsung has been working hard on building technology to improve the communication between its connected TVs and mobile devices, whether they be iOS or Android phones or tablets. Well, the company has acquired MOVL, a startup that should provide even more help in that category.
MOVL is the maker of the Kontrol.tv API platform, which lets developers create apps to connect TVs via the cloud, as well as mobile phones on home networks. The platform was fully launched last fall, after a year-and-a-half that the MOVL team spent building the system.
A representative from MOVL confirmed the acquisition with the following statement:
"In April 2013, two years after inception, MOVL has officially joined forces with Samsung. We are now a part of Samsung Electronics, and we are excited to combine our multi-screen capabilities with Samsung's scale and innovation in its device ecosystem."
MOVL has been working on the Samsung connected TV platform for a while now. The startup was one of the first winners of Samsung's Connected TV developer contests, with its WeDraw app. WeDraw enabled users to draw images through an app on their mobile phones or tablets, and have those illustrations be displayed on a Samsung TV.
But since then, MOVL has become even more ambitious, seeking to not only connect users of Samsung TVs and their mobile devices, but also to provide a singular platform upon which developers could build apps for multiple TV systems. Its Kontrol.tv interface works with both Samsung and Google TV devices, as well as iOS and Android phones and tablets.
But it was working on integration with other smart TV platforms as well. The idea was to provide one connective tissue for all phones and connected TVs, and it had six other platforms in the pipeline for later this year.
It's not clear if Samsung will continue to allow MOVL to develop for multiple TV platforms, or if it's just hoping to leverage the development platform for its own devices. The MOVL team has joined Samsung Electronics, and will be working out of the device maker's San Jose offices. In addition to the startup's 10 employees, Samsung also gets the technology platform it's built out, as well as a couple of patents pending.


SCROLL DOWN TO LOOK AT THE NOMINEE'S LIST !
Re: Fictionized Awards! VOTING IS OPEN!
And why the heck you are people nominating me?!
I blame it on there being not many others.
"Weirdest Member (In a good way)"
Thank you everyone for nominating the ones you think should be one of the nominee's.
Here's a list of which are now up for voting. You can only vote for ONE in each category.
And the same to all of the nominee's! The voting is now open, remember: You can only vote for ONE member on each category.
Voting closes on April the 11'th! So vote as soon as possible and, with your heart!
Woowww..I've missed a lot. xD Guess I should vote then.
Here's the winners of Fictionized Awards! WHEEY!
I'd like to thank my ability to be so effin' friendly. haha.
I have no idea why I won The Best Poem? But I did!
and therefore I'd like to thank whoever got me into writing poems. haha!
and I would really like to thank Mcfly!
without them I'd never met Mia, and we'd never made this site. Woo!
I would like to give a massive shout out to all of those who've voted for me!


Download the torrent file of the song of group The Unsung from album Sin Cera for free in excellent quality Lossy (MP3 320 kbps (Stereo, High Quality), AAC) and Lossless (WAVE, FLAC). Album «Sin Cera» in genre has been published 6 November 2018. The Unsung-Sin Cera.torrent download from zippyshare.


Throughout the years, Karen Herron Joiner has enjoyed refining her recipes for southern cooking for those who love delicious food, but don't have time to cook. Most of these recipes can be prepared in thirty minutes or less and require few ingredients. Family Favorites is filled with recipes and cooking secrets handed down through the generations.


Urban Pirates brings the swashbuckling experience of the high seas to the National Harbor. Its old-school pirate ship welcomes the young and young-at-heart aboard to meet the crew of buccaneers and learn a thing or two about life on the water. It hosts both family-friendly adventure cruises and adult BYOG (bring-your-own-"grog") tours of the harbor.
If you're bringing little ones along, book a family adventure cruise. When you board the boat, pick pieces for your pirate costume and let the staff decorate your biceps with buccaneer-themed tattoos. Then you'll hit the open water for about an hour, playing games and shooting water cannons at any rival pirates who get too close. If you choose the adults-only BYOG cruise, you can still get dressed up and enjoy some games. The only difference? You're invited to bring along your favorite adult beverages (coolers welcome) in cans, plastic, or glass containers.


text:
Exton is een plaats in het Engelse graafschap Devon. De plaats telt 1.399 inwoners.

Plaats in Devon


Eastern Schedule and Entry List Now Available!
We must stress that this event schedule is tentative and highly influenced by current registrations. We expect that changes will be necessary over the next few weeks as the next round of registrations begin to pour in right before the early registration fee expires August 21 (going up $100). Based upon conversations with many of you, we fully expect changes to the schedule will be required due to last minute registrations before this Aug. 21 deadline. Click here to sign up now and save money! Also if you would like to aid in our quest to provide you all with the best possible event schedule, please click now and reserve your place in the event for just $249! You can take advantage of our new Reservation option and secure your spot now at the lowest price available. Please don't wait as this option ends on August 21 as well.


text:
\section{Introduction}

The availability of deep {\em Hubble Space Telescope} surveys utilising the Advanced Camera for Surveys (ACS) and more recently Wide Field Camera 3 (WFC3) means it is now possible to routinely identify galaxies at very-high redshift, with large ($>50$) samples identified to $z\approx 8$ (e.g. Oesch et al. 2010a, Bouwens et al. 2010a, Bunker et al. 2010, Wilkins et al. 2010, Finkelstein et al. 2010, Wilkins et al. 2011a, Lorezoni et al. 2011, Bouwens et al. 2011, Lorenzoni et al. 2013, McLure et al. 2013, Schenker et al. 2013) and a few candidates now identified at $z>10$ (e.g. Oesch et al. 2012a, Bouwens et al 2012b, Coe et al. 2012, Oesch et al. 2013, Ellis et al. 2013).

While {\em Hubble} ACS and WFC3 observations (which probe the rest-frame UV continuum at $z>3$) alone allow us to learn a great deal about high-redshift galaxies, including the UV luminosity function (e.g. Oesch et al. 2010a, Bouwens et al. 2010a, Wilkins et al. 2011a, Lorezoni et al. 2011, Bouwens et al. 2011, Lorenzoni et al. 2013, McLure et al. 2013, Schenker et al. 2013), the UV continuum slope (e.g. Stanway et al. 2005, Bunker et al. 2010, Bouwens et al. 2010b, Wilkins et al. 2011b, Wilkins et al. 2013a, Bouwens et al. 2013), and UV morphologies (e.g. Oesch et al. 2010b), by combining them with {\em Spitzer} Infrared Array Camera (IRAC) photometry it is possible to also probe the rest-frame optical emission. This is extremely difficult (given the lower sensitivity of the IRAC observations) for all but the brightest individual objects. However, by stacking large samples of galaxies together it becomes possible to robustly probe the average SEDs of even the faintest galaxies (e.g. Eyles et al. 2005, Labb{\'e} et al. 2010, Gonz{\'a}lez et al. 2011, Labb{\'e} et al. 2012).

The UV/optical spectral energy distribution of a star formation dominated galaxy are affected by a complex mixture of different factors including the joint distribution of stellar masses, ages, and metallicities, dust, and nebular emission, many of which are closely coupled. The large number of effects makes it difficult to {\em ab initio} interpret observations, especially at high-redshift, where typically only broadband photometry is available, in the context of any of these individual quantities.

In this paper we use a state-of-the-art cosmological hydrodynamical simulation of structure formation ({\em MassiveBlack}-II) to investigate the UV-optical colours of high-redshift galaxies and in particular the effect of nebular emission thereupon. This paper is organised as follows: in Section \ref{sec:factors} we discuss in turn the various factors affecting the rest-frame UV/optical colours of high-redshift galaxies. In Section \ref{sec:sims} we present predictions from our large cosmological hydrodynamic simulation {\em MassiveBlack}-II. In Section \ref{sec:stellar_masses} we describe how strong nebular emission makes robust estimates of galaxy stellar masses difficult. Finally, in Section \ref{sec:c} we present our conclusions. Magnitudes are calculated using the AB system (Oke \& Gunn 1983). Throughout this work we assume a Salpeter (1955) stellar initial mass function (IMF), i.e.: $\xi(m)={\rm d}N/{\rm d}m\propto m^{-2.35}$.

\subsection{Filters used to probe the UV-optical SEDs}

Throughout this work we make use of several {\em Hubble} and {\em Spitzer} filters, including: {\em Hubble}/ACS ($B_{f435w}$, $V_{f606w}$, $i_{f775w}$, and $z_{f850lp}$), {\em Hubble}/WFC3 ($Y_{f105w}$, $J_{f125w}$, and $H_{f160w}$), and {\em Spitzer}/IRAC ([3.6] and [4.5]) filters. We also introduce four rest-frame bandpasses ($1500$\footnote{Defined as $T_{\lambda}=[0.13<\lambda/\mu m<0.17]^{5}$.}, $B$\footnote{Defined as $T_{\lambda}=[0.40<\lambda/\mu m<0.55]^{5}.$}, $V_{w}$\footnote{Defined as $T_{\lambda}=[0.45<\lambda/\mu m<0.70]^{5}$.}, and $R$\footnote{Defined as $T_{\lambda}=[0.55<\lambda/\mu m<0.70]^{5}.$})\footnote{Here we employ the Iverson bracket notation to define the bandpass, $[A]=1.0$ when A is {\em True} and $0.0$ otherwise.}. These rest-frame bandpasses allow us to consistently compare the properties of galaxies at different redshifts. The simple shape of these filters is chosen for convenience and the transmission profiles of all these filters are shown in Figure \ref{fig:filters}. Figure \ref{fig:SEDs} shows the observed frame SED of a star forming galaxy at $z\in\{5.0,5.9,6.9,8.0\}$ in relation to this filter set.

\begin{figure*}
\centering
\includegraphics[width=40pc]{figures/filters.pdf}
\caption{The transmission profiles of the various filters used throughout this study.}
\label{fig:filters}
\end{figure*}

\section{Factors affecting the UV-optical colours of star forming galaxies}\label{sec:factors}

The observed spectral energy distributions (SEDs) of galaxies are formed from the intrinsic stellar and AGN SEDs with reprocessing by dust and gas (both in the local ISM and IGM). The intrinsic SED of a stellar population (i.e. the {\em pure} stellar SED) is determined by the {\em joint} distribution of stellar masses, ages, and metallicities. To demonstrate the effect of various changes to the star formation and metal enrichment histories we utilise the {\sc Pegase.2} (Fioc \& Rocca-Volmerange 1997,1999) stellar population synthesis (SPS) model. We first, in \S\ref{sec:factors.ma}-\ref{sec:factors.Z}, describe how the rest-frame intrinsic pure stellar UV-optical $1500-V_{w}$ and optical $B-R$ colours are affected by the properties of the stellar population (distribution of masses, ages, and metallicities). In \S\ref{sec:factors.dust} we extend this to include the effect of dust and critically in \S\ref{sec:factors.neb} we discuss the effect of nebular emission.

It is also important to stress that the predicted SED, for a given IMF, star formation history, and metal enrichment history, is also sensitive to the choice of SPS model. In Appendix \ref{app:SPS} we investigate how changing the SPS model affects the predicted UV-optical colours.

\begin{figure*}
\centering
\includegraphics[width=20pc]{figures/sed_5p0.pdf}
\includegraphics[width=20pc]{figures/sed_5p9.pdf}
\includegraphics[width=20pc]{figures/sed_6p9.pdf}
\includegraphics[width=20pc]{figures/sed_8p0.pdf}
\caption{The spectral energy distribution of a stellar population which has formed stars at a constant rate for $100\,{\rm Myr}$ with $z=0.004$ at $z\in\{5.0,5.9,6.9,8.0\}$. For clarity only emission lines with $f_{x}>0.2\times f_{{\rm H}\beta}$ are shown (and only those with $f_{x}>f_{{\rm H}\beta}$ are labelled). The lower panel of each figure shows various {\em Hubble}/ACS (V$_{f606w}$, $i_{f775w}$, and $z_{f850lp}$), {\em Hubble}/WFC3 (Y$_{f105w}$, J$_{f125w}$, and H$_{f160ww}$), and {\em Spitzer}/IRAC ([3.6] and [4.5]) transmission curves. The shaded regions denote two artificial rest-frame bandpasses ($1500$ and $V_{w}$) and the two hatched regions denote the $B$ and $R$ bandpasses.}
\label{fig:SEDs}
\end{figure*}

\subsection{Distribution of stellar mass and ages}\label{sec:factors.ma}

The SEDs of individual stars vary strongly with both stellar mass and evolutionary stage (and therefore age). As such the intrinsic SED of a composite stellar population is predominantly determined by the joint distribution of stellar masses and ages. This, in turn, is determined by both the initial mass function (IMF) and the star formation history (SFH).

\begin{figure}
\centering
\includegraphics[width=20pc]{figures/combined_rest.pdf}
\caption{The predicted (using the {\sc Pegase.2} SPS code) UV-optical ($1500-V_{w}$) and optical $B-R$ (lower panel, note the difference in scale) colours as a function of the previous duration of (constant) star formation. Colours are shown for both two metallicities ($Z\in\{0.02, 0.0004\}$) and both for a pure stellar SED (dashed lines) and the SED including a nebular contribution (solid lines). The two arrows show the effect of $A_{V}=0.5$ dust attenuation (with labels denoting intermediate values of $A_{V}$) assuming the Calzetti et al. (2000) reddening law.}
\label{fig:combined_rest}
\end{figure}

\subsubsection{Star formation history}\label{sec:factors.ma.sfh}

In general, stellar populations with protracted star formation histories will contain a higher proportion of low-mass stars (as many of the original high-mass stars will have evolved off the main-sequence) causing the SED of the population to redden relative to a younger population. The sensitivity of the UV/optical colours to the recent star formation history can be seen in Figure \ref{fig:combined_rest}; this shows the sensitivity of both the rest-frame $1500-V_{w}$ (UV-optical) and $B-R$ (optical) colours to the duration of previous (constant) star formation.  Increasing the duration of previous star formation from $10\to 1000\,{\rm Myr}$ causes the pure stellar $1500-V_{w}$ colour to redden by $\sim 1.4\,{\rm mag}$. The effect on the optical $B-R$ colour is more subtle, with the colour increasing by only $\sim 0.2\,{\rm mag}$ as the previous duration of star formation is increased from $10\to 1000\,{\rm Myr}$.

Assuming an increasing SFH, which is likely to be more representative of high-redshift star forming galaxies (see for example the predictions of Finlator et al. 2011), will suppress the evolution of the $1500-V_{w}$ colour as the SED is remains dominated by the most massive stars. In contrast if we instead consider the colour evolution of an instantaneous burst over the same time period ($10\to 1000\,{\rm Myr}$) the $1500-V_{w}$ and $B-R$ colours redden by $\sim 3.5\,{\rm mag}$ and $\sim 0.5\,{\rm mag}$ respectively.

\subsubsection{Initial mass function}\label{sec:factors.ma.imf}

Changing the choice of initial mass function will also effect the distribution of stellar masses. As such it can potentially have a significant affect on the colours of a stellar population. Changes to the low-mass ($<0.5\,{\rm M_{\odot}}$) end of the IMF, have only a small effect on the shape of the SED as these stars contribute only a small fraction of the total luminosity (especially in the UV/optical) of actively star forming galaxies. On the other hand, changes to the high-mass end, will affect the mass-distribution of luminous massive stars.

The high-mass IMF can be most simply parameterised as a power law, i.e. $\xi(m>0.5\,{\rm M_{\odot}})={\rm d}N/{\rm d}m\propto m^{\alpha_{2}}$, where $\alpha_{2}$ is the high-mass slope (which for the Salpeter 1955 IMF would be $\alpha_{2}=-2.35$). Increasing $\alpha_{2}$ increases the relative proportion of very-high mass stars resulting in a bluer $1500-V_{w}$ colour, as can be seen in Figure \ref{fig:combined_rest_IMF}. Changing $\alpha_{2}$ from $-2.35$ to $-1.5$ results in the pure stellar colour decreasing by $\sim 0.2\,{\rm mag}$.

\begin{figure}
\centering
\includegraphics[width=20pc]{figures/combined_rest_IMF.pdf}
\caption{The predicted UV-optical ($1500-V_{w}$) colour as a function of the choice of IMF high-mass slope ($\alpha_{2}$) for both a pure stellar SED (dashed lines) and the SED including a nebular contribution (solid lines). In each case a metallicity of $Z=0.004$ and a $100\,{\rm Myr}$ duration of previous star formation are assumed. The vertical line denotes the Salpeter (1955) IMF ($\alpha_{2}=-2.35$).}
\label{fig:combined_rest_IMF}
\end{figure}

\subsection{Metal enrichment history}\label{sec:factors.Z}

Stars of similar mass and age with lower metallicities generally have higher effective-temperatures and thus bluer UV/optical colours (see also Wilkins et al. 2012, Wilkins et al. 2013a). A stellar population with a similar star formation history, but lower metallicity, will also then tend to have bluer UV-optical colours. This can be seen in Figure \ref{fig:combined_rest}, where the UV/optical colours ($1500-V_{w}$, $B-R$) are shown for two metallicities ($Z\in\{0.02, 0.0004\}$). While (assuming the same duration of previous star formation) the high metallicity population is always redder, the difference is sensitive to the previous star formation duration (and thus the distribution of stellar masses and ages).

\subsection{Dust}\label{sec:factors.dust}

Throughout the UV to NIR dust acts to preferentially absorb light at shorter wavelengths. One effect of dust is then to cause the observed colour to redden relative to the intrinsic colour, i.e. $(m_{a}-m_{b})^{\rm obs} = (m_{a}-m_{b})^{\rm int}+E(B-V)(k_{a}-k_{b})$ where $\lambda_{a}<\lambda_{b}$, $E(B-V)\ge 0.0$ and $k_{a}>k_{b}$. The extent of the reddening due to dust is then a product of the attenuation/reddening curve $k(\lambda)$ and a measure of the total attenuation (often expressed by the colour excess $E(B-V)$).

Assuming an SMC-like curve (Pei et al. 1992), which is favoured at high-redshift by recent observations (e.g. Oesch et al. 2012b), an optical attenuation of $A_{V}=0.4\,{\rm mag}$ (which corresponds to $A_{1500}\approx 1.76\,{\rm mag}$) will redden the $1500-V_{w}$ and $B-R$ colours by $\approx 1.36$ and $\approx 0.15$ respectively (assuming no distinction in the effect of dust between nebular and stellar emission).

If instead we assume a Calzetti et al. (2000) starburst curve (and again assume no distinction in the effect of dust between nebular and stellar emission) the same $V$-band attenuation (i.e. $A_{V}=0.4\,{\rm mag}$, which corresponds to $A_{1500}\approx 1.03\,{\rm mag}$) reddens the $1500-V_{w}$ colour by $\approx 0.63\,{\rm mag}$ and the $B-R$ colour by only $\approx 0.12\,{\rm mag}$. However, Calzetti et al. (2000) found that the nebular emission of intensely star forming galaxies is more strongly affected by dust than the stellar emission (at the same wavelength) with a the relationship between the colour excess of the nebular and stellar emission of $E(B-V)_{\rm stellar}=(0.44\pm 0.03)\times E(B-V)_{\rm nebular}$. A significant consequence of assuming the Calzetti et al. (2000) is that there is no longer a unique mapping between the intrinsic and observed colours for a given attenuation.

While in this work we are more concerned with effect of nebular emission on the intrinsic photometry it is however worth noting that the similar consequences of dust attenuation, the star formation history and metallicity make interpreting the observed broad-band colours of stellar populations in the context of these quantities extremely challenging.

\subsection{Nebular emission}\label{sec:factors.neb}

Ionising radiation, which is produced predominantly by hot, young ($<10\,{\rm Myr}$), massive stars ($>30\,{\rm M_{\odot}}$)\footnote{This also makes the presence of nebular line emission a powerful diagnostic of unobscured ongoing star formation.}, is potentially reprocessed by gas in the ISM into nebular (line and continuum) emission. At high-redshift ($z>4$), galaxy formation models (see Section \ref{sec:sims}) suggest that virtually all galaxies continue to actively form, or have recently formed, stars\footnote{Even if this were not the case it is likely that many of the galaxies currently {\em observed} (at these redshifts) would be actively forming stars by virtue of being rest-frame UV selected.}. Assuming the the escape fraction of ionising photons ($X_{f}$) is small these galaxies are likely to contain strong nebular line emission.

To include the effect of nebular emission on our predictions we use the number of ionising photons predicted (by {\sc Pegase.2}) to determine the fluxes in the Hydrogen recombination lines. Fluxes in {\em non}-Hydrogen lines are determined using the metallicity dependent conversions of Anders \& Fritze et al. (2003)\footnote{{\sc Pegase.2} can, without modification, output emission line fluxes however it does not take account variations in the line ratios due to metallicity.}. Throughout this analysis we assume that the escape fraction ($X_{f}$) is zero. This assumption allows us, when combined with the pure stellar colours, to explore the full range of potential colours.

\subsubsection{Effect on rest-frame UV-optical colours}\label{sec:factors.neb.rest}

Due to the number of strong emission lines (e.g. O[II], $H_{\beta}$, O[III], and $H_{\alpha}$) in the rest-frame optical, unless the bandpass used to probe the UV encompasses Lyman-$\alpha$, the effect of nebular emission will be to redden the UV-optical colour relative to that of the pure stellar colour. This can be seen in Figure \ref{fig:combined_rest} where both the pure stellar and the stellar with nebular emission colours are shown (as function of previous duration of star formation).

For a $100\,{\rm Myr}$ duration of previous constant star formation and $Z=0.02$, the effect of including nebular emission is to redden the $1500-V_{w}$ colour by $\sim 0.3$ (see Figure \ref{fig:combined_rest}). However, the relative effect of nebular emission changes with both metallicity and previous star formation duration. For protracted ($>1000\,{\rm Myr}$) constant star formation, the effect decreases to $\sim 0.1\,{\rm mag}$ (if there has been no star formation for $>10\,{\rm Myr}$ the contribution of nebular emission will also fall to virtually zero). This variation is predominantly due to the sensitivity to the ratio of ionising photon flux to the optical flux which is itself sensitive to the (joint) distribution of stellar masses, ages, and metallicities. The variation with metallicity is in part also due to the metallicity dependent line ratios.

The inclusion of nebular emission can (for actively star forming populations) also dramatically modify the trend with the high-mass slope of the IMF compared to the pure stellar case (\S\ref{sec:factors.ma.imf}), as can be seen in Figure \ref{fig:combined_rest_IMF}. When nebular emission is included the trend between the $1500-V_{w}$ colour and high-mass slope reverses: stellar populations with shallower IMFs (high-mass biased) have redder $1500-V_{w}$ colours. This is again a result of the increased proportion of massive hot stars which produce large amounts of ionising radiation.

\subsubsection{Redshift sensitivity and effect on observed colours}\label{sec:factors.neb.obs}

\begin{figure}
\centering
\includegraphics[width=20pc]{figures/Xch1z.pdf}
\includegraphics[width=20pc]{figures/ch1ch2z.pdf}
\caption{The predicted observed-frame X$-$[3.6] (where X $\in\{z_{f850lp}$, Y$_{f105w}$, J$_{f125w}$, H$_{f160w}\}$) and [3.6]$-$[4.5] colours as a function of redshift assuming $100$ Myr previous duration of star formation for two (stellar) metallicities ($Z=0.02$ and $Z=0.0004$). The dashed lines show the result if only stellar emission is included while the solid lines show the effect of including nebular emission (continuum and line emission).}
\label{fig:Xch1z}
\end{figure}

The effect of nebular emission on observed frame colours is critically sensitive to both the filter transmission curve and the redshift of the source. Small changes in redshift can leave strong emission lines in adjacent bands, dramatically affecting the observed colour.

This can be seen in Figure \ref{fig:Xch1z}, where the X$-$[3.6] (where X $\in\{z_{f850lp}$, Y$_{f105w}$, J$_{f125w}$, H$_{f160w}\}$) and [3.6]$-$[4.5] colours (both from the pure stellar SED and the stellar+nebular) of a young star forming stellar population ($100 {\rm Myr}$ continuous star formation) are shown as a function of redshift (Figure \ref{fig:SEDs} also shows the spectral energy distribution of a stellar population forming stars for $100\,{\rm Myr}$ along with the transmission functions of the various observed frame filters). For example, at $z=5-5.3$ there are no strong emission lines within the IRAC [3.6] bandpass, thus leaving the X$-$[3.6] colour virtually unchanged relative to that for a pure stellar SED (unless the X filter encompasses Lyman-$\alpha$). In contrast at $z<5$ and $z>5.3$ the IRAC [3.6] filter includes strong emission lines (O[III] and H$\beta$, or H$\alpha$ respectively). This results in an extremely strong sensitivity to the redshift. An increase in redshift of $0.1$ (i.e. $z=5.0\to 5.1$) can decrease the X$-$[3.6] colour by $0.5$\footnote{$z=5$ is a declining inflexion point for the X$-$[3.6] colour.} while correspondingly increasing the [3.6]$-$[4.5] colour by $0.7$. A similar situation occurs at $z\approx 7$ as the [OIII] and H$\beta$ lines move out of the [3.6] band into the [4.5] band. The [3.6]$-$[4.5] colour (which probes the rest-frame optical at $z=4-8$) also experiences significant variation as a function of redshift, as shown in the lower-panel of Figure \ref{fig:Xch1z}. Specifically, both $z=5$ and $z=6.9$ are approximately rising inflexion points, again caused by the shifting locations of the various strong emission lines.

This highlights that interpreting the observed colours of galaxies with strong emission lines is extremely challenging without precise knowledge of the redshift (or redshift distribution).

\section{Predictions from galaxy formation simulations}\label{sec:sims}

The preceding analysis demonstrated that the observed frame optical/NIR colours of high-redshift galaxies can be extremely sensitive to nebular emission. By using a galaxy formation model to predict both the star formation and metal enrichment histories we can predict the stellar spectral energy distributions (SEDs) and nebular (line and continuum) emission and thus the intrinsic observed colours.

\subsection{{\em MassiveBlack}-II}

We make use of a state-of-the-art cosmological hydrodynamic simulation of structure formation: {\em MassiveBlack}-II (for a more detailed description of this simulation see: Khandai et al. {\em in-prep}). The {\em MassiveBlack}-II simulation is performed using the cosmological TreePM-Smooth Particle Hydrodynamics (SPH) code {\sc P-Gadget}, a hybrid version of the parallel code {\sc Gadget2} (Springel 2005) tailored to run on the new generation of Petaflop scale supercomputers. {\em MassiveBlack}-II includes $N_{\rm par}=2\times 1792^{3}\approx 11.5$ billion particles in a volume of $10^{6}\,{\rm Mpc}^{3}/h^{3}$ ($100\,{\rm Mpc}/h$ on a side) and includes not only gravity and hydrodynamics but also additional physics for star formation (Springel \& Hernquist 2003), metal enrichment, black holes and associated feedback processes (Di Matteo et al.  2008, Di Matteo et al. 2012).

\subsubsection{Properties of galaxies in the simulation}

A detailed overview of the properties of galaxies (galaxy stellar mass functions, luminosity functions etc.) in the simulation is presented in Khandai et al. {\em in-prep}). Nevertheless, it is useful to present predictions for the properties which directly influence the UV-optical colours of galaxies, i.e. the star formation and metal enrichment histories.

Instead of presenting the full star formation and metal enrichment histories, in Figure \ref{fig:Age_lum.eps} we show the median mass-weighted stellar age in bins of intrinsic UV luminosity and in Figure \ref{fig:Z_lum.eps} the median mass-weighted stellar metallicity, in both cases for a range of redshifts ($z\in\{5,6,7,8,9,10\}$). The redshift trends can be seen more clearly in Figure \ref{fig:ZAge_z.eps} where the evolution of median mass-weighted stellar age and metallicity for galaxies with $-20.5<M_{1500}<-18.5$ are shown.

\begin{figure}
\centering
\includegraphics[width=20pc]{figures/Age_lum.pdf}
\caption{The mass-weighted stellar age as a function of the intrinsic UV luminosity predicted by the {\em MassiveBlack}-II simulation. The upper panel shows both a density plot (with shading denoting the number of galaxies) and the median age (and $16^{\rm th}-84^{\rm th}$ percentile range) in several luminosity bins at $z=7$. The shade of the density plot denotes the number of galaxies contributing to each bin on a linear scale. Where there are fewer than 25 galaxies contributing to each bin on the density plot the galaxies are plotted individually. The lower panel shows only the median age as a function of luminosity but for a range of redshifts ($z\in\{5,6,7,8,9,10\}$).}
\label{fig:Age_lum.eps}
\end{figure}

Figure \ref{fig:Age_lum.eps} reveals only a very weak correlation between UV luminosity suggesting any correlation in the predicted UV-optical colours is unlikely to be dominated by variations in the star formation history. Figure \ref{fig:Z_lum.eps} on the other hand reveals a strong correlation between the mass-weighted stellar metallicity and the UV luminosity. Both quantities do however show strong variation with redshift (as can be seen clearly in Figure \ref{fig:ZAge_z.eps}).

\begin{figure}
\centering
\includegraphics[width=20pc]{figures/Z_lum.pdf}
\caption{The mass-weighted stellar metallicity as a function of the intrinsic UV luminosity predicted by the {\em MassiveBlack}-II simulation. The upper panel shows both a density plot (with shading denoting the number of galaxies) and the median metallicity (and $16^{\rm th}-84^{\rm th}$ percentile range) in several luminosity bins at $z=7$. The shade of the density plot denotes the number of galaxies contributing to each bin on a linear scale. Where there are fewer than 25 galaxies contributing to each bin on the density plot the galaxies are plotted individually. The lower panel shows only the median stellar metallicity as a function of luminosity but for a range of redshifts ($z\in\{5,6,7,8,9,10\}$).}
\label{fig:Z_lum.eps}
\end{figure}

\begin{figure}
\centering
\includegraphics[width=20pc]{figures/ZAge_z.pdf}
\caption{The evolution with redshift of the simulated average (median) mass-weighted age (right-hand axis) and stellar metallicity of galaxies in the simulation with $-20.5<M_{1500}<-18.5$.}
\label{fig:ZAge_z.eps}
\end{figure}

\subsubsection{Stellar spectral energy distributions}

The stellar spectral energy distributions (SEDs) of galaxies are generated by combining the SEDs of individual star particles taking account of their metallicity and age using the stellar population synthesis (SPS) model {\sc Pegase.2} and assuming a Salpeter (1955) IMF. As noted previously, the SED predicted from a given star formation and metal enrichment history, is sensitive to the choice of SPS model. In Appendix \label{app:SPS} we consider the effect of alternative SPS models on the spectral energy distribution of galaxies predicted by the simulation.

\subsubsection{Nebular emission and dust attenuation}

Nebular emission is included in the simulated SEDs using the same prescription described in \S\ref{sec:factors.neb}. We take the ionising flux predicted from the stellar SED and determine the fluxes in the various hydrogen recombination lines assuming the escape fraction is zero. We then use the calibrations of
Anders \& Fritze et al. (2003) to determine the fluxes in the non-hydrogen lines. We also use {\sc Pegase.2} to predict the contribution of nebular continuum emission (though this is typically very small except in extreme cases). For the results presented here we do not include dust attenuation concentrating solely on the intrinsic photometry.

\subsection{Stellar colours}

The top panel of Figure \ref{fig:MB_1500V} shows the median rest-frame pure stellar $1500-V_{w}$ colour as a function of the intrinsic UV luminosity ($M_{1500,{\rm int}}$) for galaxies at $z\in\{5,6,7,8,9,10\}$. The $1500-V_{w}$ colour is correlated, albeit weakly, with the UV luminosity with the colour reddening by $\sim 0.15$ as $M_{1500,{\rm int}}=-18\to -20$ (at $z=7$). The $1500-V_{w}$ colour is also strongly correlated with redshift as can be seen more clearly in Figure \ref{fig:MB_1500V_z} where the median pure stellar colour (of galaxies with $-20.5<M_{1500}<-18.5$) is shown as a function of redshift. For example, the median $1500-V_{w}$ colour increases by $\sim 0.5$ from $z=8\to 5$.

The distribution of pure stellar colours for galaxies with $-20.5<M_{1500}<-18.5$ is shown in Figure \ref{fig:distr_colours}. The $16^{\rm th}-84^{\rm th}$ percentile range is $~0.15\,{\rm mag}$ though this increases slightly to lower redshift.

The correlation with redshift is driven by the variation in both the average star formation and metal enrichment histories of galaxies (as shown in Figure \ref{fig:ZAge_z.eps}) while the correlation with luminosity is driven predominantly by the variation in the metal enrichment history.

\begin{figure}
\centering
\includegraphics[width=20pc]{figures/1500Vw_both.pdf}
\caption{The simulated average (median) intrinsic (i.e. with no dust attenuation) rest-frame $1500-V_{w}$ colours of galaxies as a function of luminosity for galaxies at $z\in\{5,6,7,8,9,10\}$. The upper-panel shows only the pure stellar colours while the lower panel shows the average colour including the effects of nebular emission.}
\label{fig:MB_1500V}
\end{figure}

\begin{figure}
\centering
\includegraphics[width=20pc]{figures/1500Vw_z.pdf}
\caption{The redshift evolution of the median rest-frame $1500-V_{w}$ colour (points) and $16^{\rm th}-84^{\rm th}$ percentile range for both the simulated pure stellar SED and the simulated SED including nebular emission (outlined points) for galaxies with $-20.5<M_{1500}<-18.5$.  The lower panel shows the difference between the pure stellar colour and the colour including nebular emission. The dashed and solid lines show the prediction (using the {\sc Pegase.2} SPS model) assuming constant star formation since $z=15$ for the pure stellar and stellar with nebular emission SEDs respectively.}
\label{fig:MB_1500V_z}
\end{figure}

\subsection{The effect of nebular emission}\label{sec:sims.neb}

As noted in \S\ref{sec:factors.neb} the effect of nebular emission will, be adding additional flux in the $V_{w}$-band, have the result of reddening the rest-frame $1500-V_{w}$ colour relative to the pure stellar colour. This is shown for our simulated galaxies in Figures \ref{fig:MB_1500V} and \ref{fig:MB_1500V_z}.

As can be seen in Figures \ref{fig:MB_1500V} and \ref{fig:MB_1500V_z} the effect of adding nebular emission is to flatten the correlation between the $1500-V_{w}$ colour and the UV luminosity and redshift. The median $1500-V_{w}$ colour including nebular emission only reddens by $\sim 0.05$ from $M_{1500,{\rm int}}=-18\to -20$ (at $z=7$). This is because the relative strength of nebular emission is inversely correlated with both stellar metallicity and age. Those galaxies with bluer stellar colours, which are indicative of more recent star formation or lower metallicity (which are more common at higher redshift and lower luminosity) will then have stronger nebular emission and consequently will be reddened by nebular emission more than those with redder stellar colours. This has the effect of diminishing the correlation of the $1500-V_{w}$ colour with redshift and luminosity. The median $1500-V_{w}$ colour including nebular emission only reddens by $\sim 0.1$ from $M_{1500,{\rm int}}=-18\to -20$ and $\sim 0.3$ from $z=8\to 5$ (c.f. $0.1$ and $0.3$ for the pure stellar case respectively).

\subsubsection{The distribution of colours}

\begin{figure}
\centering
\includegraphics[width=20pc]{figures/dist.pdf}
\caption{{\em left-hand panels} - The distribution of both pure stellar (shaded histogram) and stellar with nebular (line histogram) intrinsic rest-frame $1500-V_{w}$ colours for galaxies with $-20.5<M_{1500}<-18.5$ at $z\in\{5,6,7,8,9,10\}$. {\em right-hand panels} - The distribution of colour residuals. In each case the vertical and horizontal lines denote the median and $16^{\rm th}-84^{\rm th}$ percentile range of the distribution respectively.}
\label{fig:distr_colours}
\end{figure}

Because galaxies with bluer pure stellar galaxies typically have lower metallicities and/or ages (and consequently stronger nebular emission) the inclusion of nebular emission reduces the scatter in the $1500-V_{w}$ colour (as measured by the $16^{\rm th}-84^{\rm th}$ percentile range), as can be seen in Figure \ref{fig:distr_colours}. At $z=8$ this reduces the scatter (as measured by the $16^{\rm th}-84^{\rm th}$ percentile range) by almost a factor of $\times 2$ while at lower redshift it is less important.

\subsubsection{The distribution equivalent widths}

\begin{figure}
\centering
\includegraphics[width=20pc]{figures/EW_dist.pdf}
\caption{The distribution of rest-frame intrinsic equivalent widths of the H$\alpha$ (left) and [OIII]$\lambda 5007$ predicted by the simulation for galaxies with $-20.5<M_{1500}<-18.5$ at $z\in\{5,6,7,8,9,10\}$.}
\label{fig:EW_dist}
\end{figure}

One alternative measure of the relative strength of nebular emission is the distribution of the equivalent widths of the prominent H$\alpha$ and [OIII]$\lambda 5007$ emission lines. These are shown in Figure \ref{fig:EW_dist} and follow a similar patten to the distribution of colour increments shown in Figure \ref{fig:distr_colours}.

\subsubsection{The effect on observed colours}

As noted in \S\ref{sec:factors.neb}, the effect of nebular emission on observed-frame colours is strongly sensitive to both the choice of filters and the redshift of the source. Even a small change in redshift can have a dramatic effect on the observed colour. Figure \ref{fig:MB_ObsC} shows the average simulated (for galaxies with $-20.5<M_{1500}<-18.5$) observed frame X$-$[3.6] and [3.6]$-$[4.5] colours for redshift ranges centred on the median redshift of observed drop-out samples (see Labbe et al. 2010, Gonzalez et al. 2011, Labbe et al. 2012): V$_{f606w}$-band drop out: $\langle z\rangle= 5.0$, $i_{f775w}$: $\langle z\rangle= 5.9$, $z_{f850lp}$: $\langle z\rangle= 6.9$, and Y$_{f105w}$: $\langle z\rangle= 8.0$. In each case the X filter is chosen (from the available {\em Hubble} ACS and WFC3 filters) such that it {\em approximately} probes the rest-frame UV continuum at $1500{\rm\AA}$. Therefore we use: $z\approx5\to$ $z_{f850lp}$, $z\approx 6\to$ Y$_{f105w}$, $z\approx 7\to$ J$_{f125w}$, and $z\approx 8\to$ H$_{f160w}$.

The trends seen in Figure \ref{fig:MB_ObsC} closely reflect those demonstrated in \S\ref{sec:factors.neb} (and seen in Figure \ref{fig:Xch1z}). We see at $z\approx 5$ and $z\approx 7$ the observed colours are particularly sensitive to the redshift, with changes in redshift of $0.1$ changing the {\em average} observed colours by up to $0.3\,{\rm mag}$.

Stark et al. (2012, hereafter S12) studied the observed frame $[3.6]-[4.5]$ colours of a spectroscopically confirmed sample of galaxies at $3<z<7$. S12 compare the $[3.6]-[4.5]$ colour distribution at $3.8<z<5.0$ (where H$\alpha$ emission, if present, will contaminate the $[3.6]$ filter) with those at $3.1<z<3.6$ (where there are expected to be no strong nebular emission lines in either the $[3.6]$ or $[4.5]$ filters) finding the $[3.6]-[4.5]$ colour at $3.8<z<5.0$ is $0.33\,{\rm mag}$ bluer than at $3.1<z<3.6$. This is interpreted as being due to the presence of nebular line emission. This closely matches our prediction at $4.5<z<4.9$ where we find the effect of nebular emission results in the observed $[3.6]-[4.5]$ colour being $0.25\,{\rm mag}$ bluer than the pure stellar colour. S12 also attempt to determine the increase in the $[3.6]$ flux due to nebular emission at $3.8<z<5.0$ by comparing the observed $[3.6]$ flux with that expected from the best fit stellar continuum models, and find an increase in the $[3.6]$ flux ($[3.6]_{\rm neb}-[3.6]_{\rm stellar}=-0.27\,{\rm mag}$) consistent with our predictions at $4.5<z<4.9$ ($[3.6]_{\rm neb}-[3.6]_{\rm stellar}=-0.29\,{\rm mag}$).

\begin{figure}
\centering
\includegraphics[width=20pc]{figures/ObsC_nobin.pdf}
\caption{The simulated observed frame X$-$[3.6] ({\em top panels}, X $\in\{z_{f850lp}$, Y$_{f105w}$, J$_{f125w}$, H$_{f160w}\}$) and [3.6]$-$[4.5] colours as a function of redshift across a narrow range centred on the snapshot redshift. The dashed and solid lines again denote the colours for the pure stellar SEDs and those including nebular emission respectively.}
\label{fig:MB_ObsC}
\end{figure}

\section{The effect on stellar mass estimates}\label{sec:stellar_masses}

We have seen that the effect of nebular emission is to typically redden the observed colour probing the rest-frame UV-optical relative to the pure stellar colour. For individual galaxies at $z\approx 7$ this can be as large as $+0.6\,{\rm mag}$ with the average at $z=6.8$ being $+0.4\,{\rm mag}$ for J$_{f125w}-$[3.6]. The effect is also strongly dependent on the redshift and choice of observed filters with changes in the redshift of as little as $\pm 0.1$ is able to change the observed colours by $>0.3\,{\rm mag}$.

Because accurate estimates of the stellar mass-to-light ratio require a measurement of the shape rest-frame UV-optical SED (e.g. Wilkins et al. 2013b) the effect of nebular emission can introduce a large bias, particularly where the redshift is not known accurately. The exact size of the effect of nebular emission on stellar mass estimates however depends on various factors including the method used to measure the mass-to-light ratio, the redshift.

As a simple illustration we consider the case where the stellar mass-to-light ratio is measured using a single colour (e.g. Taylor et al. 2012, Wilkins et al. 2013). Figure \ref{fig:MTOL} shows the relationship between the observed frame J$_{f125w}-$[3.6] colours and  J$_{f125w}$-band stellar mass-to-light ratios of galaxies at $z=6.8$ and $z=7.0$. In both cases the J$_{f125w}-$[3.6] colour is correlated with the mass-to-light ratio (though the correlation is much stronger at $z=7.0$ where the effect of nebular emission is smaller than at $z=6.8$), however, for the same observed colour the average mass-to-light ratio at $z=7.0$ is $\sim 0.25\,{\rm dex}$ ($1.8\times$) larger. That is, were the redshift erroneously assumed to be at $z=7.0$ instead of the true redshift of $z=6.8$ the stellar mass-to-light ratio would be overestimated by around $\sim 0.25\,{\rm dex}$.

\begin{figure}
\centering
\includegraphics[width=20pc]{figures/MTOL_colour_7p0.pdf}
\caption{The simulated observed frame J$_{f125w}-$[3.6] colours and J$_{f125w}$-band mass-to-light ratios of galaxies at $z=6.8$ and $z=7.0$ with $-20.5<M_{1500}<-18.5$. The two straight lines denote simple linear fits to the two sets of simulations.}
\label{fig:MTOL}
\end{figure}

\section{Conclusions}\label{sec:c}

We have explored the evolution of the rest-frame UV/optical (and observed frame near-IR) colours of high-redshift galaxies ($z=5-10$) predicted by our large cosmological hydrodynamical simulation {\em MassiveBlack}-II.

We find that the median rest-frame {\em pure} stellar UV-optical ($1500-V_{w}$) colour is correlated with both luminosity and redshift. The $1500-V_{w}$ colour reddens by $\sim 0.2$ as the luminosity increases from $M_{1500}=-18$ to $-20$ (at $z=7$) and by $\sim 0.5$ from $z=8$ to $z=5$. In both cases, this reflects the trend of increasing ages and metallicities with luminosity and to lower redshift.

However, when nebular emission is included, these correlations weaken. The $1500-V_{w}$ colour reddens by only $\sim 0.3\,{\rm mag}$ as $z=8\to 5$ and $\sim 0.1\,{\rm mag}$ as $M_{1500}=-18\to -20$. This occurs because galaxies with very blue stellar colours (indicative of galaxies with recent star formation or low metallicity) typically have stronger nebular emission causing their colours to redden by a greater relative amount.

The effect of nebular emission on observed frame colours is very sensitive to both the choice of filters and redshift. For example, at $z=7.0$, nebular emission only reddens the observed J$_{f125w}-$[3.6] colour by, on average, $\sim 0.1\,{\rm mag}$ while at $z=6.8$ it reddens the J$_{f125w}-$[3.6] colour by $\sim 0.45\,{\rm mag}$ (i.e. a difference of $\sim 0.35\,{\rm mag}$). Similarly, at $z=7.1$, nebular line emission causes the [3.6]$-$[4.5] to redden by $\sim 0.2\,{\rm mag}$, while at $z=6.8$ it causes [3.6]$-$[4.5] colour to shift blue-ward by $\sim 0.4\,{\rm mag}$ (a net difference of $\sim 0.6\,{\rm mag}$).

This strong sensitivity of observed colours to the redshift makes interpreting the colours of individual objects extremely difficult unless precise redshifts are known. Indeed, if the stellar mass-to-light ratio were inferred from the J$_{f125w}-$[3.6] colour alone a difference of $\pm 0.35\,{\rm mag}$ (as expected between $z=6.8$ and $7.0$) would roughly double

While the general trends we observe hold true irrespective of the choice of initial mass function and stellar population synthesis model both these factors can strongly affect the predicted colours. For example, utilising the Maraston et al. (2005) model yields stellar colours between $0.1-0.3\,{\rm mag}$ redder than the {\sc Pegase.2} model (which is assumed throughout this work).

\subsection*{Acknowledgements}

We would like to thank the anonymous referee for their useful comments and suggestions that we feel have greatly improved this manuscript. SMW and AB acknowledge support from the Science and Technology Facilities Council. WRC acknowledges support from an Institute of Physics/Nuffield Foundation funded summer internship at the University of Oxford. RACC thanks the Leverhulme
Trust for their award of a Visiting Professorship at the University of Oxford. The simulations were run on the Cray XT5 supercomputer Kraken at the National Institute for Computational Sciences. This research has been funded by the National Science Foundation (NSF) PetaApps program, OCI-0749212 and by NSF AST-1009781.

redpajama_set_name: RedPajamaArXiv


BLOOMINGTON, Ind. - Courseload, Inc. and Indiana University were recently recognized as gold recipients in the IMS Global Learning Consortium's Learning Impact Awards. Representatives from Courseload and IU accepted the award at the IMS Global Learning Impact 2013 conference.
The Courseload-IU eTexts and digital course materials initiative received the Learning Impact Award for its use of technology in addressing the challenges faced by the global learning community. Courseload is an innovator in the aggregation, delivery and use of eTexts and digital course materials.
"Courseload at Indiana University provides a great example of the type of world-class innovation that the Learning Impact Awards were designed to recognize," said Dr. Rob Abel, chief executive officer of IMS Global. "The net result simultaneously improves access, affordability and quality of the educational experience at Indiana University."
The Courseload platform, which has been adopted on a broad scale at IU since 2011, is currently in use by over 10,000 students in more than 250 sections.
"We're very pleased to be recognized with Courseload for leading the way on this important initiative," said Anastasia Morrone, associate vice president for learning technologies at IU. "IU's strategy for devices respects students' choices in a rapidly evolving world, while Courseload's innovations — support on any device, real-time analytics for faculty, and accessible collaboration features for users of all abilities — enable IU to decrease student costs and improve teaching and learning."
"We're very pleased to be recognized with Indiana University for this award. From our pilots in 2009 to the present, Indiana University has been a valuable partner in helping Courseload to craft a cutting-edge solution," said John Falchi, Courseload senior vice president of academic and business partnerships. "We look forward to continuing our partnership and seeing even more improvements in affordability and student success through innovation and collaboration."
Founded in 1820, Indiana University is a major public research institution with 110,000 students across eight campuses. Digital textbooks, virtual software delivery, and flexible learning environments support IU's mobile community and place the university at the cutting edge of IT for higher education. As part of this culture of innovation, Indiana University manages the nation's leading research networks, heads research initiatives supported by the National Science Foundation, partners with other universities on open source software development, and provides leadership in cybersecurity. For more about IT at IU, see http://it.iu.edu.
IU's pioneering eTexts initiative began with pilots in 2009, and finished its third full semester in spring 2013. In the last year, the number of participating course sections and students has doubled. The model is now being piloted and expanded at other institutions. For more information, visit http://etexts.iu.edu.
Driven by a commitment to increase access, lower costs and improve learning outcomes, Courseload is the leading innovator in the aggregation, delivery and use of digital course materials in higher education. Courseload eliminates the barriers that have impeded the print-to-digital evolution in academia through a business model inclusive of all stakeholders, an innovative platform incorporating study tools and analytics to enhance learning and pedagogy, and a team with deep experience in implementing educational technology solutions. Learn more at http://www.courseload.com.


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Brenda Colvin (Hardback)
Brenda Colvin (1897-1981) ranks with Sylvia Crowe and Geoffrey Jellicoe as a pioneer of twentieth-century landscape design in Britain. This first full account of her life and work demonstrates her importance. Early in her career Colvin visited the USA to see the new civic landscaping projects, especially the parkways. In England she transformed the landscapes of power stations, reservoirs, industrial sites, new towns and national parks and worked on private gardens. Her simple planting style and her ecological approach had enormous influence. Colvin championed the profession of landscape architect as a founder member and president of the Landscape Institute. Her books Land and Landscape and Trees for Town and Country remain standard works. Hal Moggridge, who became her partner; has written the foreword to this book. Trish Gibson has had full access to the archives of Colvin & Moggridge. She draws on Colvin's personal notebook and uses previously unpublished material. The offices of Covin & Moggridge continue to thrive at Little Peacocks, Filkins, Gloucestershire, where Colvin's garden is kept as it was in her day.
Biography Biography: generalHome & Garden Gardening Garden design & planningHome & Garden Gardening Gardens descriptions, history etc Publisher: Frances Lincoln Publishers Ltd Publication Date: 01/02/2011 ISBN-13: 9780711231719 Details: Type: Hardback Format: Books
Trish Gibson is a garden journalist with a regular gardening column. She is a recorder for the Cornwall Gardens Trust and editor of their journal. Her own garden is open under the National Gardens Scheme.
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Welcome to Marketing's morning briefing, a daily shot of news and a recap of the best longer reads and videos. Today we look at the UK car industry reaching a seven-year high and Argos becoming the first retailer to boast £1bn purely from mobile commerce.
Argos is the first retailer to have reached the £1bn in mobile sales in the UK over a year, according to Retail Week.
The report, taken from Argos owner Home Retail's chief digital officer Bertrand Bodson at the businesses Christmas in July event, reveals that the business did over £1bn in m-commerce last year, with sales on mobile growing 38%.
The sales figures included any sale starting on a mobile device, including deliveries to home, click and collect and reserve in store.
According to UK car industry trade body, the Society of Motor Manufacturers and Traders (SMMT), the number of cars built in the UK hit a seven year high for the first half of the year.
Some 793,642 cars were built in the UK in the first half of the year, the highest the number has been since the recession hit in 2008.
According to the BBC, the 5.4% annual rise in car production is at odds with the 7.9% decrease in UK car demand, suggesting that international trading is boosting demand and that British-made care brands are strong in key markets.
The SMMT applauded the industry's investment in technology and its relationship with government.
As part of our inaugural Marketing New Thinking Awards in partnership with Sky Media, consumer behaviour expert and author Mark 'Herdmeister' Earls, who is a member of the awards judging panel, examines Cultural Shift – one of our 12 categories. The final deadline for entries is Friday 24 July.


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The Texas Department of Motor Vehicles (TxDMV) has published in the Texas Register adopted changes to the Texas Administrative Code, which affect Deputies. Additionally, TxDMV withdrew proposed language. The adopted and withdrawal Texas Register language are attached. They are also available on the Office of the Secretary of State's website at http://www.sos.state.tx.us/texreg/pdf/backview/1003/1003is.pdf.
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