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Fifa World Cup 2022: Last Dance For Lionel Messi As Unified Argentina Ready To Give All For Their Captain
1 feared for Darwin Nunez just after his shocking miss at the tail finish of the very first half in Liverpool's meeting with Ajax. The Uruguayan's not had an easy time of it due to the fact arriving at Anfield during the summer time, immediately becoming the topic of incessant stick on social media. Every single error has been pored more than, every miss – even in national team coaching sessions – promptly gone viral. On Tuesday night, the coach promptly paid tribute to his players for "achieving our first target of the season" by getting out of "really complicated" group, but it is only correct that he's also recognised for overseeing this surprise results. On Tuesday night, in a 7-2 rout of Maccabi Haifa in which he combined sensationally with Neymar and Kylian Mbappe, the 35-year-old became the oldest player to both score and make two goals in the very same Champions League. Messi is the national team's prime scorer with 90 targets in 165 matches.
Newell's agreed to spend for his remedy, but when Argentina's financial crisis impacted the country's soccer clubs, they had been left with no decision but to reduce off their end of the bargain. Some parents even hold the identical dream for them also — el sueño del pibe. Anyway, rumours emerging immediately after school yesterday suggest that my son and his year 6 pals took it upon themselves to turn the hall into a Boxpark, by taking the lids off their water bottles and launching the contents skyward with each and every goal. It is the headteacher's fault really – he gave them the notion by singing Something Inside So Powerful ahead of kickoff. I completely agree deification of her position and claims of bravery is too significantly (fwiw I'm particular she would also agree with that).
In the summer of 2021, the then 23-year-old elevated the number of Super Eagles players in the Premier League when he signed for Watford in a deal that expense over £4 million. He went on to score 10 ambitions and assisted six additional in his debut campaign. He has played in 33 distinct finals in the blaugrana jersey, winning 24 of his 34 trophies with the team, and has scored 29 targets in them. Took one game to settle at Barça then scored in all 4 games considering that. As items stand, Lewandowski is only behind Cristiano Ronaldo and Lionel Messi in the scoring charts. It has taken the Pole nearly no time to settle in Barcelona colors following his €45 million move in the summer time.
Messi, who inherited the shirt number from Ronaldinho in 2008, donned the jersey for 13 years, scoring 630 goals just before moving to Paris Saint Germain this summer. PSG are top rated of the Ligue 1 standings with a great win record from seven games even though Montpellier are 10th. "They are a team that plays appealing football. We're expecting them to make it tricky for us." The 34-year-old Argentine forward, who joined the French club from Barcelona on a two-year contract in August, will be assessed again on Sunday — ahead of the Champions League house game against City on Tuesday. Charles Aranguiz was sent off two minutes later for the dwelling side but Paraguay could not make their late benefit count and they had their personal player sent off in the final minute when Omar Alderete saw red.
PSG.LGD will mount another attempt to claim the Aegis of Champions at this year's DOTA 2 The International . Every fan of the Chinese team wonders if this will finally be their year and, someway or the other, PSG.LGD falls a yard brief. The team's talented players will be hunting to break the curse in 2022 and some of the most significant names in the football globe have wished them luck. Following City triggered the £51m release clause in his Dortmund contract, Haaland has "loudly gone about silencing these who questioned his move to the Etihad Stadium", said Alex Brotherton in the Manchester Evening News.
Due to the fact arriving from AS Monaco, Kylian Mbappe has been PSG's most consistent aim threat. The Frenchman is regarded as the next significant factor in planet football and the all-natural heir to the throne occupied by Messi and Ronaldo more than the previous decade. His rise to prominence has been reflected in his FIFA ratings more than the years, with the lethal marksman getting continuous upgrades. Lionel Messi and Cristiano Ronaldo have dominated the globe of football for over a decade, sharing all the accolades and awards amongst them and causing an endless debate about who the greatest of all time is.
Lionel Messi is normally spoken of as maybe the game's greatest player ever, but he's under no circumstances lifted the well-known gold trophy for his country, Argentina. It is a continual source of criticism for the man nicknamed La Pulga Atomico, the atomic flea, due to his compact stature and the way he buzzes past defenders. His determination to swat aside these complaints may well be all the greater when you contemplate that the 35-year-old's identity as an Argentino has been questioned simply because he left the country as a teenager to commence his ascent to stardom in Spain. That's the inspiration behind the new NPR podcast La última copa – The Last Cup – which is out now, hosted by Jasmine Garsd. The partnership with Sorare adds to a slew of notable deals between sports stars and crypto platforms. French soccer player Kylian Mbappe and American tennis legend Serena Williams have previously announced tie-ups with Sorare.
Ionel Messi and Cristiano Ronaldo could make history by becoming part of a pick group of players who have managed to participate in as several as 5 Planet Cup competitions. Each Argentina and Portugal have clinched qualification to the 2022 Globe Cup, one particular which will take location in Qatar in November and December, and the two stars are expected to feature in the competition if they remain healthy. Liverpool forward Mohamed Salah has thrust himself into the conversation for the world's best player title with spectacular targets and performances handful of playing the game could match. "For a player to have a great rating, he really will have to have had a good game," Dangoumau explains.
Messi's major wages could be fulfilled by the Premier League side and he could be tempted to reunite with Guardiola for 1 final push in his profession. It remains to be noticed no matter whether the Spanish gaffer can convince Messi to lastly play in the Premier League and prove his high-quality in the greatest football league in the planet. Leo was a perfect fit for Guardiola's possession-primarily based, tiki-taka model and scored 91 ambitions in 2012, the majority of which he played under the Spaniard. If Messi becomes offered subsequent summer season, Manchester City could look to make a swoop for him. Having a player with such experience and high quality would surely give them the boost they have to have to dominate Europe. Gerd Muller will really feel challenging carried out by but Beckenbauer is one of the greatest defenders to have ever played the game.
She can be noticed rocking an all-black workout outfit and a black cap, though also flauting her Christian Dior handbag. The casual side of the 35-year-old forward, who is normally camera-shy and rarely shares personal images on social media, is visible through the summer season break. While some veterans are at the major of the list, it is only natural that footballers' abilities and performances dwindle with age.
The Portuguese star averages a hat-trick every 18.9 games played, according to MessivsRonaldo.app. He has scored 44 hat-tricks for True Madrid, 3 for Man Utd, 3 for Juventus and ten for Portugal. Paris Saint-Germain forward Messi opened the scoring in Argentina's opening World Cup game against Saudi Arabia in group C. On the other click here for more info hand, the Argentines suffered a enormous shock as Saudi went on to win the game two-1. Brand Finance further claim the loss of Messi will lead to "diminished fan perceptions", with "the club's global following at danger of shrinking". On Saturday, Messi held an emotional press conference to confirm he is ending his 21-year association with FC Barcelona.
SEOUL, Nov. 23 — About 600 police personnel will be deployed for crowd handle in Gwanghwamun Square in central Seoul where thousands of sports fans are expected to gather … A Texas lady allegedly set her boyfriend's family house on fire and FaceTimed him to show off the blaze soon after assuming he was cheating on her, police mentioned. Breaking News A gunman has opened fire on a Walmart division retailer in Chesapeake, Virginia, with police saying there are "multiple fatalities" as well as wounded individuals at the scene.
So far this campaign, Messi has 14 assists in 18 matches for PSG coming at an typical of .84 per 90 minutes. Last season also saw Messi struggle to convert his probabilities compared to usual, scoring 11 times across Ligue 1 and the Champions League from 16.68 Expected Objectives . For reference, the Argentine maestro netted just six occasions across 26 Ligue 1 games final term. PSG travelled to Corsica with out suspended pair Neymar Jr. and Sergio Ramos, but they still place a strong XI out at the Stade François Coty. That didn't stop Ajaccio from possessing the initially chance of the game, although, with Mounaïm El Idrissy hitting the outdoors side-netting of Gigio Donnarumma's goal (5′). Messi then curled a totally free-kick towards the Ajaccio target which deflected off Bevic Moussiti-Oko, but Benjamin Leroy reacted nicely to make the save (13′).
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Zeppola is a typical Italian dessert that they prepare in various regions in Italy during the carnival period. In south Italy is a typical dessert for the feast of San Giuseppe, at 19th of March, so is widely known as Zeppola di San Giuseppe.
In Caiazzo a 19th of March, in all the shop/markets of Aulo Attilio Caiatino offered to the people Zeppola di San Giuseppe.
The main ingredients are flour, sugar, eggs, butter and olive oil, custard, a sprinkling of icing sugar and cherries in syrup for decoration. It can be fried or baked it depends to the region. Both are tasty! Zeppola is covered with pastry cream with on top of the cherries in syrup and dusted with icing sugar.
We are more than four months here in Italy and I could say that I am in love with Italian kitchen/gastronomy. What I loved the most is the simplicity. Getting involved with Italian Culture is one of the aims of our EVS project. When this interaction has to do with food, we have one more reason to get involved. Also whet we also appreciate the most here in Caiazzo is that they try to keep some local customs in their pure and original way. We could say that Zeppola di San Giuseppe is one of these traditions that they keep alive and practice them until today.


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ARRIVAL -- Blu-ray Review by Porfle
There are at least two kinds of sci-fi movies that I love. One is the slam-bang space opera with explosions in space, spaceships having dogfights in space, and/or space monsters destroying the world before returning to outer space. These are awesome and I wouldn't dream of looking down my nose at them because they're just so much dumb fun.
The other kind of sci-fi movie I love is the kind that's good because it's just so much smart fun. Movies such as 2001: A SPACE ODYSSEY, THE ANDROMEDA STRAIN, DEEP IMPACT, and CONTACT. I love them because they present scintillating scenarios and ideas which are often both illuminating and, in the best cases, mind-expanding. And they explore these things in relation to how they would affect humanity in the really-real world.
With ARRIVAL (2016), you get all that in addition to the kind of intensely emotional situations that can only exist in science fiction.
Upon the arrival of 12 massive egg-shaped spaceships which park themselves over various locations around the world, linguistics expert Louise Banks (Amy Adams, THE MASTER, SUNSHINE CLEANING, STILL STANDING) is pressed into service by the government to help establish contact with the aliens, an experience that will dovetail in ways she can't yet imagine with the tragic death of her daughter Hannah, whom we see in fleeting flashbacks.
Director Denis Villeneuve turns this into a gorgeously-photographed dreamlike journey for her and us in which we're never really able to recover from the disorienting unreality of the situation.
The hard-edged military protocol of the base camp adjoining one of the ships (embodied by Forest Whitaker's no-nonsense "Colonel Weber") and all the scientific mumbo-jumbo that's thrown around only serve to make Louise's entry into the mysterious craft and her attempts to communicate with its ultra-strange occupants seems even more breathlessly surreal.
Memories of her daughter keep haunting her throughout the experience, visions which are seemingly unstuck in time as Louise is drawn into the aliens' non-linear concept of past, present, and future. Scenes of her inside the cavernous spaceship, interacting with her otherworldly counterparts on an increasingly emotional level, are among the most compelling and thought-provoking of any I've seen in any sci-fi film.
In addition to this ARRIVAL deals in a fascinating way with the catastrophic effects such an event would have on humanity on a global scale. Much of this is conveyed by news reports of violent societal upheaval (without, for once, a bunch of CNN personalities playing themselves badly) and the growing paranoia of various government leaders who are inching toward war against the outworlders.
The juxtaposition between the genuine desire for peaceful understanding and empathy shown by Louise and her science-expert cohort Ian (Jeremy Renner, "Hawkeye" in the AVENGERS movies) and the increasingly hostile attitude displayed by Earth's military leaders is jarring.
It also leads to some of the film's most suspenseful and disturbing moments, especially when a mutinous faction within Colonel Weber's own ranks devises a plot to sabotage the ship.
But despite the dramatic urgency of this global countdown to interplanetary war, much of the story is devoted to diligent cerebral research and detective work along with Louise's own intense emotional journey through the whole experience and how profoundly it changes her life.
Amy Adams is a joy to watch as she fully inhabits the role of the pensive yet passionate Louise, with Jeremy Renner providing capable support as Ian. Forest Whitaker (THE MARSH, PAWN, CATCH .44, HURRICANE SEASON), of course, is pretty much a national treasure by now and can do no wrong.
SPFX are as fine as modern CGI can devise, but it's the full-scale ship interior that's most impressive. I won't go into the appearance of the aliens or the nature of their written language, which both Louise and Ian struggle mightily to make sense of, but both are sufficiently bizarre. All other aspects of the production are first-rate.
The Blu-ray from Paramount Home Media Distribution is widescreen with Dolby 5.1 stereo in English, French, and Spanish and subtitles in English. Also included is a download code for a digital HD copy. Bonus features consist of lengthy featurettes (over 80 minutes total) including "Xenolinguistics: Understanding 'Arrival'", "Acoustic Signature: The Sound Design", "Eternal Recurrence: The Score", "Nonlinear Thinking: The Editing Process", and "Principles of Time, Memory, and Language."
ARRIVAL is slow and thoughtful, but continuously fascinating--it never lags or loses interest for those serious sci-fi lovers who are truly along for the ride. And the ending delivers the kind of thought-provoking yet deeply emotional payoff that should leave them contemplating certain mysteries of life, love, and the universe for some time to come.
Buy it at Amazon.com:
Blu-rayUHD/BD/Digital HD Combo
Blu-rayBD/Digital HD Combo
http://www.ArrivalMovie.com/
Twitter: https://twitter.com/ArrivalMovie
Facebook: https://www.facebook.com/ArrivalMovie
Instagram: https://www.instagram.com/ArrivalMovie
iTunes: http://j.mp/ArrivalWebsite
Posted by Porfle Popnecker at 10:17 PM
Labels: aliens, Blu-Ray, DVD, HD-DVD, movie, Paramount, Porfle, review, sci-fi, science fiction
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redpajama_set_name: RedPajamaCommonCrawl


Express Highlights, also known as SDE (same day edits), are very common in weddings and they are normally used to display the morning activities leading up to the actual wedding.Most of the time, if you have engaged any of our videography partners, RekordHaus or Miror Creations, or any of your preferred videographers, their package usually comes with SDE.
We would normally encourage the wedding couple to use the videographer's highlights as they usually have more comprehensive coverage and tend to be more entertaining. However, if you do not have a videographer, we would be most glad to help and put together an Express Highlights reel for you too!
The main goal of our Express Highlights is to keep your guests entertained. Most of the time, we will try our best to incorporate some video footage too.
If you would like to view more SDE samples, do contact us to arrange for an appointment with our friendly people.


In the mid-twentieth century, some of the nation's concert halls experienced financial challenges and fell into disrepair as the orchestras they incubated moved on to other performing locations.
In the face of the New York Philharmonic's move to newly-constructed Lincoln Center, Carnegie Hall in New York City was nearly demolished in 1960. Fortunately, the Citizens Committee for Carnegie Hall, headed by violinist Isaac Stern and other influential New Yorkers, persuaded the State of New York to purchase Carnegie Hall. They then formed a nonprofit to restore Carnegie Hall to the glory it now experiences.
The Musical Fund Hall, which was the Philadelphia Orchestra's first home in the 19th century, faced a similar fate in the mid-20th century. Although Musical Fund Hall was not demolished, unlike Carnegie Hall, it no longer hosts concerts. Rather, in 1981, a developer (which I will call the "MFH Developer") purchased Musical Fund Hall and redeveloped it as condominiums.
Historical articles about Musical Fund Hall's redevelopment don't describe the developer's financing structure. So, using the Musical Fund Hall's redevelopment as an example, this blog will examine how the financing might have looked.
MFH Fund– owns Musical Fund Hall, provides equity, and uses the funds from the Construction Loan to pay for the restoration and construction. The MFH Fund also will sell the condo units.
Condo Mortgage Lender–the MFH Fund and Real Estate Broker might team up with a mortgage lender to facilitate mortgage loans for condo buyers. This may or may not be the same as the Construction Lender.
A capital stack includes all debt and all forms of equity that used to finance the project. Let's assume that the MFH Developer utilized a typical capital stack involving a construction loan (let's assume 60-65% of the cost). The rest of the redevelopment would be funded with equity. The MFH Developer might provide about five percent (5%) of the equity. The remaining equity would come from outside investors into a real estate development fund (which we will call the MFH Fund).
If there is a plan to presell as many condo units as possible, there might be two classes of equity in the MFH Fund. The first would be a shorter-term, preferred class redeemable as deposits for pre-sales of condo units are received. The remainder of the equity would be a common class. The common equity would only be redeemed after completion of construction and final sale of the condo units.
Construction Loan (60-65% of capital stack)–the Construction Lender will provide a mortgage loan to MFH Fund to redevelop Musical Fund Hall. Although the loan documents and mortgage for the full amount would be signed before the reconstruction starts, typically Construction Lender will only disperse funds from the Construction Loan as work is completed. This not only protects the Construction Lender from a disreputable developer, but it also can benefit MFH Fund. Typically, interest will not accrue on Construction Loan funds until they are dispersed.
The Construction Lender would receive only payments of principal and interest on the Construction Loan. The Construction Lender would not otherwise share in profits from the development.
Preferred Equity in the MFH Fund (5-10% of capital stack)–the MFH Fund might have a preferred class of equity. Preferred equity in real estate funds may be used in lieu of a short-term mezzanine or bridge loan. Here, Preferred Equity might provide temporary financing for anticipated pre-sales of condominium units.
Preferred Equity typically receives only a fixed return plus return of its capital. It is called preferred equity, because it is paid before the Common Equity holders receive their return. Unlike Common Equity holders (described below), Preferred Equity holders would not otherwise share in the profits from the project.
The Preferred Equity would be redeemed using deposits from condo pre-sales. The ratio of Preferred Equity to Common Equity would depend upon the project's underwriting.
Common Equity in the MFH Fund from outside investors (19%-28% of capital stack)–The bulk of the equity likely would be common equity. Like Preferred Equity, Common Equity typically receives a minimum return and return of its equity. Common Equity also typically receives a percentage of any profits from the project after all capital has been returned. The remainder of the profits would go to the MFH Developer for its "carried interest" (described below). If condominium sales do not go as well as planned, it is the Common Equity holders who stand the most to lose, but they also have the most to gain if things go well.
Equity in MFH Fund from MFH Developer (2%-6% of the capital stack)–Most Construction Lenders require that the project developer contribute at least five percent (5%) of the equity. MFH Developer likely would acquire Common Equity. If the Common Equity investors include a private equity fund, MFH Developer's equity might be subordinate to the Common Equity.
MFH Developer carried interest (0% of capital stack)–The carried interest isn't part of the capital stack. MFH Fund's carried interest would entitle it to receive percentage of the profits with the Common Equity holders once all capital has been returned.
MFH Developer might receive payments on its carried interest before return of capital to the Common Equity holders. If so, there probably would be a "clawback." A clawback would require MFH Developer to pay back any amounts it received if Common Equity holders otherwise would not receive return of their capital.
Most development projects are set up to build or renovate a project with a goal of selling it for a profit. For tax purposes, the real estate (condo units) is considered akin to "inventory." It is not considered real estate held for business or investment purposes.
Income from the sale of the condo units will be taxed at ordinary income rates, rather than capital gains rates.
Because the real estate is not held for business or investment purposes, it is not eligible for deferral of the gains upon sale under Section 1031.
Likewise, payments to MFH Developer due to its carried interest also will be taxed as ordinary income.
However, all is not lost under the tax code. Since MFH Fund would be considered a partnership for tax purposes, the MFH Fund is the classic "pass-through" entity under the tax law. As such, investors in the MFH Fund likely will be eligible for a tax deduction equal to 20% of their income from the fund, provided the MFH Fund meets certain criteria.
Don't Try This at Home on Your Own!
This is just a case study of a possible real estate development capital stack and real estate fund. These are complex transactions, which require specific expertise in real estate, finance, tax, and securities law. Plus, each project has its own, unique, needs, which should be incorporated into the structure.
However, properly structured, a real estate development project can save a historic property like Musical Fund Hall, help to revitalize a city through provision of walkable housing, and also make money for the developer and investors involved.
DISCLAIMER: The content of this blog is for informational purposes only and does not provide legal advice to any person. No one should take any action regarding the information contained in this blog without first seeking the advice of an attorney. Neither reading this blog nor communication with Whitman Legal Solutions, LLC or Elizabeth A. Whitman creates an attorney-client relationship. No attorney-client relationship will exist with Whitman Legal Solutions, LLC or any attorney affiliated with it unless and until a written contract is signed by all parties and any conditions in such contract are fully satisfied.
 Music Fund Hall opened on December 29, 1824 by the Musical Fund Society. It was the site of many important political events, as well as music concerts and authors. Violinists Ole Bull, Camillo, and Henri Vieuxtemps and singers Jenny Lind and Henrietta Sontag all appeared there in the 19th century. Marquis de Lafayette attended a reception in his honor there in 1825. In 1837, Pennsylvania's first Constitutional Convention was held there, and in 1856, the first Republican national convention was held at Music Fund Hall. Charles Dickens, Ralph Waldo Emerson, and Arthur Conan Doyle all spoke there.
 Musical Fund Hall was purchased by a developer in 1980, after decades of decline into a dilapidated condition. See Musical Fund Hall by Sarah Carroll on Phila Place. After the renovation, Musical Fund Hall lost its Landmark designation from the National Park Services, but it continues to be listed on the National Register of Historic Places. See National Park Service website for more information.


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Home Blog OpenStack project status August
OpenStack project status August
8 September 2014 by Jeroen Bakker in OpenStack
A wrap-up of some of the things our OpenStack team has been up to in the past month.
Our OpenStack project team is currently working with a number of environments. We've got several testing platforms, for both administrators working on building the final product and internal users beta testing functionality and working on how-to's and tutorials.
Our developers and administrators have been rigorously testing our (erasure coded) Ceph storage platforms, looking for the best way to configure everything for optimal performance results. Although our Ceph platform will be based on SSD infrastructure, we still want to ensure that the configuration of the software allows optimal utilization of the full performance potential.
Some other examples of what we've been working on include:
Failover and recovery mechanisms and live migration
Service automation using the (public) API
Streamlining installations with Puppet and Razor
Data collection and reporting (from Ceph) in Calamari
Our default test set of OS images that can be used has been expanded and now includes CentOS, Ubuntu, CoreOS, CirrOS and Windows 2012. Every image has a slightly different method to get them to work for the user, and our colleagues are preparing to write up clear instructions for all.
Last month also saw the first real work on the visual branding of the final product. We're working on logos and icons for the service, the website and our supporting user community. For those curious, we've included some sketches below.
We've also opened up a sign-up possibility for public beta testing of the project. Currently we're still in the internal test stage, but once we've declared the platform stable enough, we'll contact those who've shown an interest.
Follow our latest news and stay tuned on our technological developments. By reading our blog, you'll get to know the people behind our services. Furthermore you'll find fun insights and everything else that keeps us busy.


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3. She was his girl, he was her boyfriend She'd be his wife and make him her husband A surprise on the way, any day, any day One healthy and little giggling, dribbling baby boy The wise men came, three Indeed, the abrupt change at 3:13 in the track 'Sysyphus (Part 4)' caused the only music-induced jump scare I've ever seen. 1. The song's title is actually "Thnks fr th Mmrs", so the answer's spelling should be changed, and the proper title should also be accepted. List the title of the song. (Love Me Like Music) I'll Be Your Song by Heart (1976) 98. 1. David Geddes' "Run Joey Run". Check out our popular trivia games like Songs with Body Parts in the Title, and Title in the Lyrics Quiz #1 And for more musical absurdity, check out the 30 Funniest Funniest Rap Lyrics Walking On Thin IceYoko Ono. Start the wiki, Javascript is required to view shouts on this page. Level 45 . Put quotation marks around song titles: For best appearance in professionally typeset material, use proper typographical quote marks and apostrophes (curly quotes). "Folkin' Around" (Panic! Songfacts category - Songs with initial titles. Man's "Keep On Crinting". Songs are ranked based on an inverse point system, with weeks at No. 26 March 2020, 18:03 | Updated: 3 April 2020, 14:07. This quiz is about some of them. I'm So Lonesome I Could Cry. At The Disco are well known for having hilarious and long-winded song titles. And while many artists opt for song titles that look good etched into a Grammy, others just want to have a good laugh. by Ray Conniff on album The Christmas Day Brings Memories - 100 Titles. For example, A Doll's House or Raging Bull. Click to copy. List of 1,355 words that are 3 letter words.Add length, consonants, vowels, syllables, origin, spelling and more. Boy - The Magic Numbers. Several rock bands have written songs with a woman's name in the title and some of the songs have gone onto become huge hits. If you reference more than one song on the album in your paper, simply cite to the album as a whole in your bibliography. 1. So, why is this song in The Beatles' songs list? Songs with letter in the lyrics are only allowed if that word is in the song's name as well....more. 2. Thanks! CEO. List of 30 words that are 3 letters and adjectives. NCT 2020 Logic Puzzle 258 #1 Artists of the 2000s 159; Crossword Beatles Lyrics 124; The Devil is in the Detail - Top of the Pops 118; 3 Composers Grid 92; Musical Groups in Comic Books 90; The age of pithy pop extends beyond just the one-word hits; the average length of a Hot 100 song title has shrunk from 3.76 words in the 1960s … Here is another quiz on some great Beatles' songs. Beach Music Songs with 2 Word Titles #1 Love: Almost Mine: Amazingly, Amazing: At Last: Beach Fever: Beach Trip: Beach Vacation: … 5/11/2015. Add italics to the title of an album, a play, a film, or a television series. Ana - Pixies. Dio - Tenacious D. Dog - El Perro Del Mar. (1970s) 1; 3 Letter Words in 2000s Songs 1; Top User Quizzes in Music. Learn to ultimate word find. Created by mk87 on 09 Feb 2018. Aug 3, 2016. Five-letter song titles: Clip #5 by scarequotes published on 2011-06-27T17:02:41Z. Can you pick the correct three-letter word missing from these 2010s song titles? Find two word song titles tracks, artists, and albums. Before you say some of these songs are not beach music, I am gonna to qualify them. Ada - the national. If you are citing the title of a music album, you would use italics. Dazu gehört der Widerspruch gegen die Verarbeitung Ihrer Daten durch Partner für deren berechtigte Interessen. Songs with cry in the lyrics are only allowed if that word is in the song's name as well....more. More Cry Wolf #57 of 134 The Best Songs About Crying #10 of 78 The Best Songs With Wolf in the Title. Yahoo ist Teil von Verizon Media. Booyah Achieved by Minus The Bear (2002) "WHAT'S YOUR FAVORITE SONG TITLE?" Pete Parada (The Offspring): I Just Don't Think I'll Ever Get Over You by Colin Hay (1998) Copied to clipboard. Enjoy. 2. They're not the only ones though, as many bands and singers have ushered in fun new songs with even better song titles. Recording information on songs is not always available, or not accurate enough to state a specific year of recording. This list includes all songs known to be written by Prince (regardless of official credits, and/or whether a studio recording is known to exist). "The Boy Who Blocked His Own Shot" (Brand New) 2. Ann - Stooges. 4. Songs are a way of expression that sets the mind free. 3. Jingle Bells. For all the the psychedelic exploration before and after, 1969 release Ummagumma is, to my mind, the strangest entry in their discography. In this case, the year will be followed by a *. Three letter words. Level 54. Readers recommend playlist: songs with one word titles A reader picks a list from your nominations – songs from Santana, Grateful Dead and Soulsavers all making the cut Scott Blair The following is a list of all songs recorded and performed by the Swedish pop group ABBA, alphabetised by the English title of the song. Use this tool to have your song titles correctly capitalized. The remaining songs titles left on each teams' list are worth one point each. Since I like different types of songs, and since I'm half Asian (and stereotypically like math and numbers), I decided to compile a list of awesome songs with numbers in their title. The song titles that I chose were based off of several factors: Thought Provoking Word Combinations Visual Imagery Humor General Creativity Connection to Events […] This will take you to a list of links to CD and/or MP3 product pages from one or more online merchants that have sound samples. L. Let It Snow. Say My Name-Destiny's Child Subject: Re: THREE Word Song Titles! Five-letter song titles: Clip #4 by scarequotes published on 2011-06-27T17:02:41Z. Three different songs with this title, by Frankie Goes to Hollywood, Huey Lewis and Jennifer Rush, were in the charts in the same year, 1985. Beatles' Three-Word Song Titles 10 question trivia quiz, authored by mrgrouchy. Do you know anything about this type of music? 0. Song titles in foreign languages should be left in that language if it is popularly known that way and capitalized according to the rules of that language. The three remaining Beatles never did a proper version for Anthology 3, 'cos George (Harrison) didn't wanted to record another Lennon solo. 15. 228 posts latest by Veljko Dragićević 3 hours ago We can all use a little help from our friends when we run into issues on Genius, so here's the hub to ask Annotation Review In the Source Column, G means the topic was at the Guardian, SB means it was at the Song Bar. 97. Sie können Ihre Einstellungen jederzeit ändern. Find the latest in two word song titles music at Last.fm. Other released songs. This will take you to a list of links to CD and/or MP3 product pages from one or more online merchants that have sound samples. A new version of Last.fm is available, to keep everything running smoothly, please reload the site. Some user-contributed text on this page is available under the Creative Commons Attribution-ShareAlike License; additional terms may apply. Popular Music: Groups / Bands - 3 letters. Three letter words. 1. If an opposing team has the same title in their list, both teams need to cross that song out from their list. Some of my favourite songs in English language from A to Z. For example, Nina Simone Live in Paris. From country to emo, these artists aren't afraid of their fans having a few chuckles at their expense, as evidenced by these hilarious song titles. Five-letter song titles: Clip #3 by scarequotes published on 2011-06-27T17:02:41Z. 26. It's The Most Wonderful Time Of The Year. 13. Connect your Spotify account to your Last.fm account and scrobble everything you listen to, from any Spotify app on any device or platform. Song Titles: For All We Know - Friendship Train. Dies geschieht in Ihren Datenschutzeinstellungen. With the use of texts, emails, and conversations through social media, there really isn't any art in the process of writing a letter. It Came Upon A Midnight Clear. You searched for Popular Music: Groups / Bands with 3 letters and pattern = ??? Music Quiz / 3-letter + 4-letter song titles Random Music or Song Quiz Match the artist in the clue to the song title containing only a 3-letter word followed by a 4-letter word. Let There Be Peace On Earth. This page gives a list of song titles beginning with T that were radio hits from the 1960s through the early 1970s (1960-1975). e.g. After The Love Has Gone - Earth Wind & Fire That's not a grammar rule but it is a good design and printing rule. Leave feedback. Wir und unsere Partner nutzen Cookies und ähnliche Technik, um Daten auf Ihrem Gerät zu speichern und/oder darauf zuzugreifen, für folgende Zwecke: um personalisierte Werbung und Inhalte zu zeigen, zur Messung von Anzeigen und Inhalten, um mehr über die Zielgruppe zu erfahren sowie für die Entwicklung von Produkten. View word search examples. Test your knowledge on this music quiz and compare your score to others. Why are the examples a bit obscure? UPS. 1. Four Letter World. J. Jingle Bell Rock. To find other songs by a band or artist listed on this page, click on a name. All of the songs listed have the word letter in the song title. To listen to a song clip, click on a song title below. Go directly to shout page. By Jason Lipshutz. Für nähere Informationen zur Nutzung Ihrer Daten lesen Sie bitte unsere Datenschutzerklärung und Cookie-Richtlinie. List of songs with lyrics, meanings, interpretations and chart positions starting with L. Ok this is very random but this is a love letter composed of song titles hope you enjoy My homie, lover, friend, we have had our good times and our bad times.Once upon a time we made the decision to separate and while we were apart I realized that none else comes close to making me feel the way that you do. Average score for this quiz is 5 / 10. Song titles listed in music programs may not be placed in quotation marks. 3-letter 4-letter 0.026 • About NamePlayground.com • Contact NamePlayground.com NamePlayground.com is a participant in the Amazon Services LLC Associates Program, an affiliate advertising program designed to provide a means for sites to earn advertising fees by advertising and linking to Amazon.com. Song Title Hijinks! 30. How many people actually write a letter in the age of technology?
3 letter song titles
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3 letter song titles 2020


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\section{Introduction}

Diffuse interstellar bands (DIBs) are ubiquitous absorption lines detected in the reddened stars, which originate from foreground interstellar clouds.
Recent surveys have discovered over 500 DIBs in the near-UV to near-infrared (NIR) wavelength range \citep{jen94,hob08,hob09}. DIBs have also been found in extragalactic objects such as the Magellanic Clouds \citep{wel06, cox07}, M31 \citep{cor11}, and high-$z$ damped Lyα systems \citep{law08}.

Although no DIB carriers have been identified successfully, organic compounds based on carbon atoms mostly contribute to  absorption features \citep{sar08}.
In particular, polycyclic aromatic hydrocarbons (PAHs) are expected to be possible carriers of DIBs because they are rich and stable even in harsh interstellar environments, where the molecules are exposed to UV photons \citep{sar08}.
However, despite recent progress in spectroscopic studies of such molecules in the laboratory, no PAHs have been assigned to any DIBs yet. \citet{cla03}, \citet{sal11}, and \citet{gre11} could not detect the absorption lines of some neutral PAHs in the near-UV spectra of stars; they derived the upper limits of the abundances of some specific neutral PAHs.

DIBs in the NIR wavelength range are essential for testing the PAH-DIB hypothesis because
the electronic transitions of ionized large-sized PAHs are thought to fall in the NIR wavelength range \citep{mat05,rui05}. If the DIB carriers are identified as PAHs, we will be able to better understand the variety and abundance of specific PAHs in interstellar clouds, which will eventually allow us to study the formation and destruction processes of such organic material in the universe. Owing to the recent progress in NIR high-resolution spectroscopy, the number of discovered NIR DIBs has recently increased rapidly. \citet{geb11} detected 13 new DIBs in the $H-$band toward the Galactic center.
\citet{cox14} reported 11 NIR DIB candidates in $0.9 < \lambda < 2.5\mu$m detected in their spectral survey of NIR DIBs with the X-Shooter spectrograph on the Very Large Telescope (VLT). They showed that some of these candidates are detected near the wavelength of the electronic transitions of ionized PAHs from the matrix isolation experiments of \citet{mat05}. However, as \citet{cox14} noted, the NIR spectra of gas-phase PAHs in the laboratory are needed for identification.
The NIR wavelength range is also useful in exploring the DIBs toward heavily reddened stars because of its higher transmittance in interstellar clouds compared to the optical wavelength range \citep{geb11, zas14}.

In addition to the spectroscopic studies of molecules in the laboratory, for the identification of the carriers it is also important to constrain the physical properties of the DIB carriers in the astronomical environment. For this purpose, the correlations among the strength of DIBs and the amount of other atomic or molecule species in the gas clouds have been extensively investigated for the DIBs in the optical wavelength range \citep{kre87,cam97,mcc10,fri11}. Regarding the NIR DIBs, although earlier studies succeeded in detecting new DIBs, their properties in the interstellar clouds have not been investigated owing to small sample size \citep{job90, cox14}.

In this study, we present the first comprehensive survey of NIR DIBs in the $z-$, $Y-$ and $J-$bands with the newly developed NIR Echelle WINERED spectrograph \citep{ike06,yas06,yas08,kon15} mounted on the Araki 1.3 m Telescope in Japan. WINERED offers a resolution of $R = 28,300$ with high sensitivity in wide wavelength coverage of $0.91-1.36 \mu$m, which is critical for detecting and surveying weak DIBs. DIBs in this wavelength range have not been searched systematically for many lines of sight \citep{job90,foi94,cox14}. We constructed the largest data set so far of NIR high-resolution spectra for 25 reddened early-type stars, and we investigated the correlations among the NIR DIBs detected herein, strong optical DIBs in the literature, and the reddening of stars. The rest of the paper is organized as follows. In \textsection{2}, we describe our observations, targets, and the data reduction procedures. In \textsection{3}, the search for NIR DIBs is described. In \textsection{4}, the properties of the identified DIBs are described. In \textsection{5}, we discuss the correlations among reddening, NIR DIBs, and optical DIBs. In \textsection{6}, we discuss the carrier properties of several DIBs. We present a summary of this study in \textsection{7}.

\section{Observation, Targets, and Data Reduction}

We used the newly developed high-resolution NIR Echelle spectrograph, WINERED \citep{ike06,yas06,yas08,kon15}, mounted on the F/10 Nasmyth focus of the Araki 1.3 m telescope at Koyama Astronomical Observatory, Kyoto-Sangyo University, Japan \citep{yos12}. WINERED uses a 1.7 $\mu$m cutoff 2048 $\times$ 2048 HAWAII-2RG array with a pixel scale of $0''.8$ pixel$^{-1}$, simultaneously covering a wavelength range $0.91-1.36\mu$m. We used a slit $48''$ in length and $1''.6$ (2 pix) in width, which corresponds to a spectral resolution of $R=28,300$ or $\Delta v = 11$ km s$^{-1}$.

Bright early-type (O, B, A) stars with $J < 6.2$ mag were selected as targets
 (Table \ref{targets}). The color excesses of the targets are in the range $0.07 < E(B-V) < 0.85$ except for Cyg OB2 No.12 ($E(B-V) = 3.4$).
 We also obtained spectra of Rigel ($E(B-V)=0.0$) as a reference, which should not show any absorption features due to interstellar dust.
Observations of almost all targets were conducted from 2013 November to 2014 January. Only two stars (Cyg OB2 No.12 and HD190603) were observed in 2012 July when we used an engineering array with worse sensitivity, in particular at shorter wavelength ($\lambda < 1\mu$m), compared with that of the currently used scientific array. Therefore, the signal-to-noise ratio (S/N) and quality of the spectra of these stars are not as good as the other data. The telescope was nodded by about 30 arcsec along the direction of the slit length between alternating frames to offset the sky emission. Only for HD 37043, which is embedded in the Orion Nebulae, were the frames obtained without nodding, and corresponding sky frames were obtained in a field far from the star to avoid the emission from the Orion Nebulae.

All the data were reduced using standard procedures with IRAF, including sky subtraction, flat fielding, the extraction of spectra, and wavelength calibration with Argon lamp spectra. For the correction of telluric absorption lines, we obtained the spectra of the A0V standard stars without reddening at an airmass similar to those of the targets (Table \ref{targets}). The spectra of the targets were divided by those of the standard stars to remove telluric absorption lines. Note that we did not remove the hydrogen and metal absorption lines in standard stars, because the profile fitting and removal of those features is difficult in many cases owing to contamination of atmospheric absorption lines. Therefore, emission-like features appear in the divided spectra. The telluric absorption lines by water are stronger for two stars, HD190603 and Cyg OB2 No.12, than for the other stars because these two stars were observed in July, when the humidity is very high in Japan. The spectra are normalized by a low-order Legendre function using the IRAF task, \textit{continuum}, for each order of Echelle spectra.

\section{The Search for DIBS}

In our wavelength range, four major DIBs are known at $\lambda = 9577, 9633, 11797, \text{and }13175$\r{A} \citep{job90,foi94}. In addition, \citet{gro07} found a DIB at $\lambda =$10780\r{A}, which is correlated with $E(B-V)$. We first searched for these five DIBs in the target spectra. Although $\lambda \lambda$9577 and 9633, which are proposed to be the electronic transitions of the fullerene cation \citep[C$_{60}^+$;][]{foi94,jen97,gal00}, are detected toward some reddened stars, their EWs cannot be estimated confidently because of heavy telluric absorption lines. Conversely, the fairly strong DIBs, $\lambda \lambda$10780, 11797 and 13175, are detected toward many lines of sight. In addition to these five major DIBs, three weak DIBs at $\lambda = 9017, 9210, \text{and }9258$\r{A} were reported in the Orion Nebulae by \citet{mis09}, who suggested that these DIBs are additional features of C$_{60}^+$. Because the DIBs, $\lambda \lambda 9210 \text{and } 9258$, which fall in our wavelength range, are blended with stellar absorption lines, it was difficult to evaluate their EWs without modeling the stellar spectra. The ``C$_{60}^+$'' DIBs in the wavelength range of WINERED, $\lambda \lambda 9210, 9258, 9577, \text{and }9633$, will be discussed in a separate study after a complete evaluation of the contamination by the overlapped telluric and stellar absorption lines.

Subsequently, we searched for new DIBs in the wavelength range of $0.91 < \lambda < 1.32 \mu$m. Note that the wavelength ranges $0.93 < \lambda < 0.96 \mu$m,  $1.11< \lambda < 1.16\mu$m, and $\lambda > 1.32 \mu$m were not usable in searching for DIBs owing to heavy telluric absorption lines. We searched for the absorption lines satisfying the following two criteria: 1) the absorption lines are detected with a 5$\sigma$ level in the spectra of  reddened stars, and 2) the absorption lines do not exist in the spectra of the reference star Rigel or the model stellar spectra of the A0Ia, A0V, B5Ia, and B5III stars. We synthesized model spectra using the SPTOOL program \citep{tak95}, which employs ATLAS9 model atmospheres \citep{kur93}.\footnote{The atomic line data was adopted from the Vienna Atomic
Line Database \citep[VALD; ][]{kup99}.
The effective temperatures and surface gravities are as follows : $(T_\text{eff} , \log
g)=(9900,2.1)$ for A0Ia, (9727,4.27) for A0V, (13600,2.5) for B5Ia, and (15000,4.22) for B5III. These values are adopted from \citet{gra92} ($T_\text{eff}$ of  A0V and $\log g$ of A0V and B5V), \citet{gra09} ($T_\text{eff}$ of A0Ia and B5V), and \citet{cox00} ($\log g$ of A0Ia and B5Ia).}
We first searched for such absorption lines in the spectrum of HD20041, because even weak DIBs are expected to be detectable toward HD20041 in view of the high S/N of the spectrum and the large EWs of $\lambda \lambda$11797 and 13175.
Then, we searched for absorption lines in the spectra of other stars that are detected near the wavelength of the absorption lines detected toward HD20041.
Consequently, 15 absorption features were detected toward multiple lines of sight as new DIB candidates.

To confirm that the candidate absorption features are DIBs originating from the interstellar clouds, we checked the consistency between the velocity of the intervening gas clouds and those of the detected absorption features. The rest-frame wavelengths of the absorption features were determined by fitting Gaussian profiles to the absorption features detected toward HD20041 (see the next section for details). As for the stars toward which the interstellar atomic absorption lines (\ion{K}{1}, \ion{Na}{1}, and \ion{Ca}{1}) have been reported in the literature (see the Table \ref{targets} footnote for references), we compare the velocities of the detected absorption lines we detected with those of the atomic absorption lines. Regarding the other stars without known interstellar atomic lines, we compare the velocities of the candidate absorption lines with those of the confirmed DIB $\lambda 11797$. The absorption lines whose velocities are inconsistent with those of the interstellar clouds should be categorized as non-DIBs.
However, no absorption features were rejected by checking their velocities. Because their EWs do not show any dependence on the stellar spectral types but exhibit positive correlations with $E(B-V)$ (see \textsection{5.1}), we conclude that all of the absorption features are truly DIBs.

In summary, we identified 15 new DIBs in addition to five DIBs previously identified in this wavelength range. Table \ref{DIBs} summarizes all the DIBs detected. The table also shows the effect of the stellar and telluric absorption lines on the DIBs. Figures \ref{DIBspec1}- \ref{DIBspec4} show the DIB spectra for all observed stars.
The EWs of all DIBs toward all observed stars are summarized in Table \ref{DIBew1}. We calculated the EWs by a simple integration because the DIB profiles are not well established. Only for DIB $\lambda 10504$, whose EWs cannot be evaluated by simple integration because of blending with stellar lines (see \textsection{4.3.1} for details), we fit Gaussian profiles to the DIB profile to estimate the EWs. The wavelength range used for the integration is arbitrarily set to include the whole DIB region (see Figures \ref{DIBspec1}-\ref{DIBspec4}). The uncertainties of the EWs ($\sigma _{\text{err}}$) or 5$\sigma$ upper limits (EW$_{\text{upp}}^{5\sigma}$) are estimated from the S/N of the neighboring continuum using the following equations:
\begin{align}
\sigma _{\text{err}}  &= \Delta \lambda \sqrt{w} (\text{S/N})^{-1}, \\
EW _{\text{upp}}^{5\sigma} &= 5 \Delta \lambda \sqrt{w_{\text{inst}}} (\text{S/N})^{-1},
\end{align}
where $\Delta \lambda$ is the wavelength interval per pixel ($ \sim 0.2$ \r{A}), $w$, and $w_{\text{inst}}$ are the widths of the DIB and the instrumental profile in pixels, respectively. Here, $w_{\text{inst}}$ is defined as $2J + 1$ pixel, where $J(=2 \text{pixels})$ is the slit width used in our observation.
We did not consider additional systematic uncertainties due to continuum fitting, telluric absorption lines, and stellar lines. Several concerns on the systematic uncertainties in the EWs of each DIB will be discussed in \textsection{4.3}.

Recently, \citet{cox14} reported 11 new NIR DIB candidates with their NIR DIB survey with VLT/X-shooter, 8 of which fall in our wavelength range, although they could not confirm that the candidates are truly DIBs because they detected the candidates only toward 3 stars at most. Of their candidates, 7 are included in our newly identified 15 DIBs for which
we confirmed that they are truly DIBs by detecting them toward many lines of sight. Note that a line at $\lambda \sim$10507\r{A}, which is reported as a DIB candidate by Cox, is identified as a stellar absorption line of \ion{N}{1} in this study. The DIB λ10792 was originally reported as an unidentified line by \citet{gro07}.

\section{Properties of NIR DIBs}

\subsection{EW Distribution}

Figure \ref{ewdist} shows the distribution of the ratios of the EWs to $E(B-V)$ for DIBs in 4000 \r{A} $< \lambda < 18000$ \r{A}. The data for optical DIBs in the wavelength range 4000 \r{A}$< \lambda < 10000$\r{A} are adopted from the catalog published on the Web\footnote{http://leonid.arc.nasa.gov/DIBcatalog.html} by P. Jenniskens. The catalog is primarily based on the studies by \citet{jen94} and \citet{kre95} (see the Web site for other references). We do not include the recent surveys of DIBs in the optical wavelength range such as \citet{tua00,hob08,hob09} in this figure, because most of the DIBs found in these surveys are weak. The data for $H-$band DIBs are adopted from \citet{cox14}. Because the authors do not show the ratios of EWs to $E(B-V)$, we roughly estimated them by dividing the EWs toward 4U 1907$+$09 by the color excess, $E(B-V) = 3.48$. Regarding the DIBs identified in this study, we determine the ratios of EWs to $E(B-V)$ by fitting linear functions ($EW = a \times E(B-V) + b$) to EW$- E(B-V)$ plots (see \textsection{5.1} and Table \ref{ebvcc}). From Figure \ref{ewdist}, we found that the NIR DIB $\lambda 13175$ is one of the strongest DIBs ever detected. We also found that there are many DIBs in the range $0.91\mu\text{m}< \lambda < 1.32\mu$m, in which only five DIBs were previously confirmed. All of the DIBs detected herein are stronger than 10 m\r{A}, below which the majority of optical DIBs are distributed. Assuming a similar distribution to that of the optical DIBs, we expect that the number of weak NIR DIBs increases by an order of magnitude through deeper spectroscopic observations.

\subsection{Wavelength and FWHM}

We measured the rest-frame wavelengths in air ($\lambda _0$) and FWHM of all identified DIBs by fitting Gaussian functions to profiles. We fitted the Gaussian functions to the profiles of HD20041, toward which almost all DIBs are detected with high S/N. Because the DIB $\lambda 12293$ toward HD20041 is blended with two \ion{N}{1} stellar absorption lines, we used the spectrum of HD21389 only for this DIB. Table \ref{DIBs} summarizes the fitting results, and Figure \ref{profilefitting} shows the spectra of the DIBs and fitted Gaussian profiles. We shift the measured wavelength to the rest-frame wavelength using the heliocentric velocities of the strongest velocity component of the interstellar clouds toward these stars (Table \ref{targets}).
The systematic uncertainties may remain in the measured $\lambda _0$ and FWHMs of the DIBs because of the possible velocity dispersion of multiple velocity components toward these two stars.

\subsection{Comments on Individual DIBs}

\subsubsection{$\lambda \lambda$10360, 10393, 10438, and 10504}

These DIBs fall in the wavelength ranges without any telluric absorption lines. Because the S/N of raw spectra is higher compared with the S/N of spectra divided by that of telluric standard stars, their EWs are calculated from the undivided spectra. DIB $\lambda 10504$ is contaminated by two stellar lines: \ion{Fe}{2} $\lambda 10501.5$ emission line of supergiant stars of early A-type and late B-type and \ion{N}{1} $\lambda 10507.0$ absorption line of stars earlier than late B-type (Figure \ref{profilefitting}). In the case when the relative velocity between the background star and the interstellar clouds is large, the observed DIB is blended by the lines. A relative velocity of only $\sim 30$ km s$^{-1}$, which produces a wavelength shift of $\sim 1$\r{A}, can affect the calculation of EWs of the DIB. In this study, we do not calculate the EWs of the DIB toward HD50064 and HD223385, which are clearly detected but significantly blended by the stellar lines (see Fig \ref{DIBspec2}). When the DIB is separately detected with slight blending, we calculate the EWs by fitting two Gaussian profiles to the blended DIB profile and \ion{N}{1} absorption line (Figure \ref{DIBspec2}). We do not estimate systematic uncertainties from the fitting procedure. For a more precise analysis of this DIB, a model spectrum that reproduces both the absorption and emission lines for each star is required.

\subsubsection{$\lambda 10697$}

The DIB $\lambda 10697$ is surrounded by strong stellar absorption lines of \ion{C}{1} and \ion{Si}{1} as well as telluric absorption lines (Figure \ref{profilefitting}). Because these stellar metal absorption lines are also detected in the A0V telluric standard stars, many false emission-like features appear in all telluric-corrected spectra. These artificial features significantly affect the continuum fitting and evaluation of EWs or upper limits. Therefore, we attempted to remove from the telluric standard spectra the \ion{C}{1} lines at $10689.72, 10683.03, 10691.24, \text{and }10707.32$\r{A} and the \ion{Si}{1} lines at 10685.34 and 10694.25\r{A}.

First, we define the instrumental profile of stellar metal absorption lines using the absorption profile of \ion{S}{1} 10459.41\r{A} and \ion{Si}{1} 10827.09\r{A} lines, which are free from any blending of telluric absorption lines and show a clear line profile. The profiles of \ion{S}{1} 10459.41\r{A} and \ion{Si}{1} 10827.09\r{A} lines are used for the removal of \ion{C}{1} and \ion{Si}{1} lines, respectively.
We then fit the instrumental profiles to the \ion{C}{1} and \ion{Si}{1} lines by shifting the wavelength and scaling the intensity on the basis of the intensity ratios of the metal absorption lines in the model spectra of A0V stars.
We construct a spectrum containing only \ion{C}{1} and \ion{Si}{1} absorption lines by synthesizing the profiles of each absorption line.
These stellar metal lines are removed from the telluric standard spectra by dividing them by the synthetic spectra of \ion{C}{1} and \ion{Si}{1} lines. Note that the slight residuals appear to remain in the resultant spectra for some telluric standard stars probably because the \ion{S}{1} line profile is slightly different from the \ion{C}{1} lines.
Finally, telluric absorptions are corrected using the \ion{C}{1} and \ion{Si}{1} corrected spectra of telluric standard stars. Consequently, the continuum fitting is improved except for Cyg OB2 No.12 and HD190603, for which the data were obtained in 2012 July (when the climate is humid in Japan), and the metal absorption lines of the telluric standard star HIP87108 could not be removed well because of the low S/N and quite strong telluric absorption lines. Figure \ref{DIBspec2} shows the spectra of $\lambda 10697$ divided by the spectra of telluric standard stars, from which the \ion{C}{1} and \ion{Si}{1} absorption lines were removed. The EWs of $\lambda 10697$ are estimated, but the upper limit of the EW is not evaluated  because of the possible residual of stellar metal lines when the DIB is not detected.

\subsubsection{$\lambda 12293$}

The DIB is located between two \ion{N}{1} absorption lines, $\lambda \lambda$12289.18 and 12298.54 (Figure \ref{profilefitting}). Because of the relatively large wavelength offset $\sim5$\r{A} ($\sim120$ km s$^{-1}$), it is unusual that they are blended significantly. However, these stellar lines affect the determination of the continuum level around the DIB. In particular, the DIB of HD20041 is surrounded by both the \ion{N}{1} absorption lines and false emission-like features from the \ion{N}{1} absorption lines in the telluric standard star. Although the DIB itself is clearly detected toward HD20041, we cannot estimate its EW.

\subsubsection{$\lambda 12799$}

Because the DIB is located in the wings of the strong and broad \ion{He}{1} and \ion{H}{1} (Pa $\beta$) absorption lines, we remove these broad lines by fitting a high-order polynomial function with an IRAF task (i.e., \textit{continuum}) for telluric-corrected spectra (Figures \ref{DIBspec3.5} and \ref{profilefitting}). Although we do not consider various possible systematic uncertainties, we can identify this absorption as a DIB because of a clear positive correlation with $E(B-V)$ (see \textsection{5.1}). Note that the upper limit of the EWs for the DIB cannot be evaluated for Rigel, HD38771, and HD37043 because the telluric absorption lines cannot be removed sufficiently well.

\section{Correlations}

To reveal the properties of the DIB carriers in an astronomical environment, it is a first step to investigate the correlations among DIBs as well as the correlations of DIBs with the parameters of interstellar clouds, such as reddening \citep{her93, cam97, fri11}. The correlations of the NIR DIBs at $\lambda > 1\mu$m have been discussed for a limited number of lines of sight \citep{job90, geb11, cox14} except for the strongest DIB in the $H-$band, $\lambda 15272$, which was examined by \citet{zas14} for about 60,000 lines of sight in the SDSS-III/APOGEE survey. Here, we analyze the correlations among the NIR DIBs that we identified at $0.91< \lambda < 1.32 \mu$m, $E(B-V)$, and optical DIBs, with a significant number of lines of sight (i.e., 25) for the first time. The EWs of the optical DIBs are adopted from \citet{fri11}, who investigated the correlations among eight strong optical DIBs ($\lambda \lambda$5487.7, 5705.1, 5780.5, 5797.1, 6196.0, 6204.5, 6283.8, and 6613.6). Among the 25 stars that we observed, the optical spectra of 19 stars were also obtained in \citet{fri11}. Therefore, it is possible that the correlation between optical and NIR DIBs can be investigated using a significant number of lines of sight.

\subsection{Correlations with $E(B-V)$}

Figure \ref{ebvcc1} show the EW$-E(B-V)$ plot. We also plot the data of \citet{cox14} for the DIBs that they detected. However, we do not include their data in the calculation of the correlation coefficients in order to preserve the uniformity of data. We fit the linear functions ($EW = a \times E(B-V) + b$) to each EW$-E(B-V)$ plot. The results are summarized in Table \ref{ebvcc}.
In the calculation of the correlation coefficients, we exclude the data point of Cyg OB2 No.12, for which the EWs of the optical DIBs are known to be much lower than that expected from the correlation with $E(B-V)$ \citep{chl86}. To compare the correlation coefficients with those of the optical DIBs, we also show the correlation coefficients between $E(B-V)$ and the EWs of the eight optical DIBs taken from \citet[][; Table \ref{ebvcc}]{fri11}. To eliminate the bias effect and the difference in sample size, we calculate the correlation coefficients using only the 19 stars observed in both NIR (our data) and optical wavelength ranges \citep{fri11}. As an example, Figure \ref{ebvcorr_rep} shows the correlations of the optical DIB $\lambda 5780.5$ and the NIR DIB $\lambda 11797$ with $E(B-V)$.

All NIR DIBs are found to have a positive correlation with $E(B-V)$, which is expected for DIBs.
We focus on the DIBs detected toward more than 10 lines of sight, whose correlation coefficients appear to be reliable.
The correlation coefficients of all the NIR DIBs are found to be lower than those of the eight strong optical DIBs calculated for the same sample ($r \sim 0.9$). When discussing the difference between two correlation coefficients, we must consider the attenuation of the correlations due to measurement errors and the statistical significance of the difference between correlation coefficients. Here, we will consider whether the differences in the correlation coefficients between optical and NIR DIBs are statistically significant. We focus on the correlation coefficients of three NIR DIBs, $\lambda \lambda 10780, 11797, \text{and }13175$, because they are detected toward many lines of sight ($>10$) and the uncertainties of their EWs are expected to be low owing to their large EWs and the smaller effect of contamination by stellar lines. Regarding the other DIBs, statistical tests are not meaningful because of the limited sample size and/or large systematic uncertainties.

We conduct a statistical test for the pairs of the three NIR DIBs and eight optical DIBs to clarify the difference between the correlation coefficients using the Fisher $z$-transformation. Consequently, the correlation coefficients of the five optical DIBs with $r>0.91$ are found to be different from those of the three NIR DIBs, with a 95\% significance level. Therefore, the difference in the correlation coefficients with $E(B-V)$ between the optical and NIR DIBs are suggested to be statistically significant for some pairs. As for the other pairs and NIR DIBs, further observations are necessary.

The high correlation coefficients of optical DIBs show that the abundances of their carriers are simply in proportion to the amount of gas in the lines of sight. Considering the lower correlation coefficients of NIR DIBs,
we infer that the abundance of the NIR DIB carriers is more sensitive to other physical parameters of the interstellar clouds (such as ionization UV flux) as well as to the amount of gas in the line of sight.

\subsection{Correlations among NIR DIBs: A Family of NIR DIBs?}

We also examine the correlations between all pairs of NIR DIBs except for 5 weak DIBs, which are detected toward fewer than 10 stars, and 2 DIBs $\lambda \lambda 12293 \text{ and }12799$, whose EWs have large systematic uncertainties owing to a blending of neighboring stellar absorption lines. From the NIR DIB set identified, we search for so-called families, in which DIBs are well correlated with each other. DIBs in a family are expected to arise from molecules having similar physical and/or chemical properties \citep{mou99,mcc10}.

The correlation coefficients for all 55 pairs consisting of 11 DIBs are shown in Table \ref{nirdibcc}.
As in the previous section, we do not include the EWs of DIBs toward Cyg OB2 No.12 in the calculation. All pairs are found to have positive correlation coefficients. In particular, three pairs consisting of $\lambda \lambda 10780, 10792, \text{and }11797$ have the highest correlation coefficients with $r\sim0.95$, suggesting that these DIBs can be classified as a family (Figure \ref{NIRcorrelation}). Because all three DIBs are fairly strong and detected toward over 10 lines of sight, the correlation coefficients should be reliable. Note that $\lambda 13175$ is also well correlated with the three DIBs $\lambda \lambda 10780, 10792, \text{and }11797$, but the correlation coefficients ($r\sim 0.9$) are slightly lower than those among the three DIBs.
Because there are several points that do not quite fit the correlation, carriers of these three DIBs would not be the same molecule. Note that $\lambda 10792$ toward Cyg OB2 No.12 is considerably weaker than that expected from the correlations (Figure \ref{NIRcorrelation}), suggesting that the carrier of this DIB may become less abundant due to some chemical processes, which would be efficient in a dense cloud with $n_\text{H} \sim 10^3$cm$^{-3}$ \citep{cas05}. Alternatively, the high X-ray flux from many massive stars in the Cygnus OB2 association including Cyg OB2 No.12 may affect the abundance of the $\lambda 10792$ carrier \citep{gre01}.

Two pairs, $\lambda 10504 - \lambda 12623$ and $\lambda 10504 - \lambda 13175$, are also found to have high correlation coefficients of $r>0.95$ (Figure \ref{NIRcorrelation2}). However, the correlation coefficient of the remaining pair, $\lambda 12623 - \lambda 13175$, is lower ($r=0.84$). This is because the EWs of $\lambda \lambda 12623 \text{ and }13175$ toward HD50064, whose EW of $\lambda 10504$ cannot be measured owing to the blending of the stellar absorption lines (see \textsection{4.3.1}), do not match the correlation. As the number of lines of sight used for the calculation of the correlation coefficients is small for these pairs (e.g., seven stars for the $\lambda 10504 - \lambda 12623$ pair), the correlation coefficients could be affected by the sample selection. Although these DIBs may form another family in view of the high correlation coefficients, it is necessary to increase the data points to confirm this from more solid correlations.

\subsection{Correlations of NIR DIBs with Optical DIBs}

Finally, we examine the correlations between the optical and NIR DIBs. We focus on four NIR DIBs, $\lambda \lambda 10438, 10780, 11797, \text{and }13175$, whose correlation coefficients with optical DIBs can be calculated with over 10 data points. Regarding the other DIBs, the number of data points available for the calculation of the correlation coefficients is too small for a statistical discussion. As in the previous two sections, we exclude Cyg OB2 No.12 from the calculation of the correlation coefficients. Table \ref{optcc} shows the correlation coefficients of 32 pairs consisting of 8 optical DIBs and 4 NIR DIBs. As a reference, we also calculate the correlation coefficients among optical DIBs using only the stars observed by us and \citet{fri11}.

\citet{fri11} showed that the correlation coefficients of all pairs consisting of eight optical DIBs have $r>0.9$, except for the two pairs $\lambda5487.7 - \lambda 5797.1$ ($r=0.87$) and $\lambda 5797.1 - \lambda 6283.8$ ($r=0.86$). The correlation coefficients calculated in this study for the optical DIBs are as high as theirs for all pairs. However, none of the correlation coefficients between NIR and optical DIBs are found to be as high as those among optical DIBs, suggesting that these NIR DIBs do not form a family with the optical DIBs. This is consistent with the discussion in \textsection{5.1}, in which a clear difference in the correlation coefficients with $E(B-V)$ between optical and NIR DIBs is shown.

In addition, we find that the three strongest NIR DIBs, $\lambda \lambda 10780, 11797, \text{and }13175$ are better correlated with $\lambda \lambda 5705.1, 5780.5, 6204.5, \text{and }6283.8$ ($r=0.8 - 0.9$) than with $\lambda \lambda 5797.1, 6196.0, \text{and }6613.6$ ($r=0.6-0.7$) although there are a few exceptions such as $\lambda 5705.1 - \lambda 13175$ ($r=0.75, N=10$), whose correlation coefficient is lower compared to those of $\lambda 5705.1 - \lambda 10780$ and $\lambda 5705.1 - \lambda 11797$. Figure \ref{NIROPTcorrelation} shows the correlations between four NIR DIBs and two representative optical DIBs in the two groups, $\lambda \lambda 5780.5 \text{ and } 5797.1$. The DIB $\lambda 10438$ is moderately well correlated with the eight optical DIBs (correlation coefficients are $\sim$0.7-0.8). Because the DIB $\lambda 10438$ is weaker than the other three DIBs, the correlation coefficients could be affected by the relatively large uncertainty of the EWs.

These two groups of optical DIBs classified by their correlation with NIR DIBs are consistent with the previous studies on the correlations among optical DIBs. \citet{cam97} showed that two pairs of $\lambda \lambda 5780.5, 6204.5$ and $\lambda \lambda 5797.1, 6613.6$, which are members of the groups, are well correlated. $\lambda \lambda 6196.0, 6613.6$ is the only pair that is proposed to have a perfect correlation \citep{mou99,mcc10}.
However, the differences in the correlation coefficients between the two groups are not statistically significant. For all pairs, we cannot exclude the null hypothesis that the correlation coefficients are not truly different. For example, the probability that the two correlation coefficients of $\lambda 5780.5 - \lambda 10780$ ($r=0.85, N=17$) and $\lambda 5797.1 - \lambda 10780$ ($r=0.70, N=15$) are not different is estimated to be $p=0.32$, which is too high to reject the null hypothesis.
Therefore, it is necessary to increase the number of samples to clarify the difference in correlation coefficients.

\section{The carriers of NIR DIBs}

\subsection{Cation Molecules}

In \textsection{5.3}, we suggested that $\lambda \lambda 10780, 11797, \text{and }13175$ are better correlated with $\lambda \lambda 5705.1, 5780.5, 6204.5, \text{and }6283.8$ ($r=0.8 - 0.9$) than with $\lambda \lambda 5797.1, 6196.0, \text{and }6613.6$ ($r=0.6-0.7$).
Among the optical DIBs, the environmental dependencies of two representative DIBs in the two groups, $\lambda \lambda$5780.5 and 5797.1, have been extensively investigated \citep{kre87, cam97, vos11, fri11}. The ratio $\lambda 5797.1 / \lambda 5780.5$ depends on the local UV intensities of the clouds because of the different ionization potentials of the DIB carriers \citep{cam97, vos11}. \citet{cam97} suggested that the ionization potential of the $\lambda 5791.1$ carrier is lower than that of the $\lambda 5780.5$ carrier. On the basis of modeling of the photoionization equilibrium, \citet{son97} estimated the ionization potential of the $\lambda 5797.1$ carrier as $\sim$ 11 eV, whereas they suggested that the $\lambda 5780.5$ carrier is a cation molecule according to its high ionization potential. The stronger correlations of the three NIR DIBs with $\lambda 5780.5$ rather than with $\lambda 5797.1$ may show that their carriers are also cation molecules with ionization potentials as high as the $\lambda 5780.5$ carrier, probably ionized PAHs. It is also suggested that the other weaker NIR DIBs that are well correlated with the three strongest DIBs $\lambda \lambda 10780, 11797, \text{and }13175$, such as $\lambda \lambda 10504, 10792, \text{and }12623$ are also from cation molecules (see \textsection{5.2}).

In our sample, HD23180 ($E(B-V)=0.31$) and HD24398 ($E(B-V)=0.32$) have high $\lambda 5797.1 / \lambda 5780.5$ ratios of $\sim$0.7-0.8, suggesting that the clouds toward these stars are $\zeta -$type, meaning that the UV intensity is weak relative to the cloud density \citep{vos11}. We compare the EWs of NIR DIBs in the $\zeta -$type clouds with those toward two stars with similar $E(B-V)$, HD2905 ($E(B-V) = 0.33$) and HD24912 ($E(B-V)=0.33$), whose $\lambda 5797.1 / \lambda 5780.5$ ratios are $\sim 0.3$, which is near the threshold for the classification of $\zeta-, \sigma-$type clouds.
$\lambda 5780.5$ in $\zeta -$type clouds is weaker than those toward HD2905 and HD24912 by a factor of two to three although their color excesses are almost the same. This can be interpreted as the results of the $\lambda 5780.5$ carrier decreasing in $\zeta -$type clouds, where the molecules are shielded from the UV flux. From our results, the NIR DIBs, $\lambda \lambda 10780, 11797, \text{and }13175$, in $\zeta -$type clouds are also found to be weaker than those toward HD2905 and HD24912 by a factor of three to four, which is similar to the factor of $\lambda 5780.5$. This similar dependence on the UV intensity also illustrates that the carriers of $\lambda \lambda 10780, 11797, \text{and }13175$ and $\lambda 5780.5$ may have similar ionization potentials.

\subsection{Carrier Candidates}

We showed that a considerable number of DIBs are widely distributed in the NIR wavelength range as in the optical wavelength range. A number of ionized large-sized carbon molecules are proposed to have the transitions in the NIR wavelength range, which is consistent with our suggestion that the carriers of some NIR DIBs are cation molecules. First, ionized buckminsterfullerenes (C$_{60}^+$ and C$_{60}^-$) are also suggested to have transitions in the NIR wavelength range from the laboratory experiment \citep{ful93}. In fact, DIBs $\lambda \lambda 9577$ and 9633 are expected to be the transitions of C$_{60}^+$ \citep{foi94}. Next, ionized PAHs (cation and anion) are theoretically suggested to have lower-energy transitions in the NIR wavelength range \citep{sal96,rui05}. \citet{mat05} obtained the absorption spectra of some ionized PAH molecules in the NIR wavelength range. Recently, \citet{jon13} proposed that heteroatom-doped (e.g., Si, O, N, and S) hydrogenated amorphous carbons (a-C: H: X) can be the DIB carriers. However, there is no strong evidence of any of those candidates of NIR DIB carriers. Further observational constraints on DIB properties as well as the identification with NIR absorption spectra of the proposed molecules in the laboratory are necessary to reveal the carriers of NIR DIBs.

The NIR absorption spectra of 27 ionized PAHs (cations and anions) are obtained by \citet{mat05} using the matrix-isolation technique. \citet{cox14}, who explored the DIBs in the NIR wavelength range, compared their newly detected DIB candidates and the electronic transitions of ionized PAHs. They found that some of the NIR DIBs are detected within a few tens of angstroms from the wavelengths of the strong electronic transitions of ionized PAHs reported by \citet{mat05}. Among the eight NIR DIB candidates that are confirmed as DIBs in this study, they suggested that wavelengths of $\lambda \lambda 10393, 10438, 10504, 10780, \text{and }13027$ are near those of strong bands of singly ionized PAHs. Among the eight NIR DIBs newly detected in this study, the DIB $\lambda 10792$ is detected close to the wavelength of the strong electronic transition of C$_{42}$H$_{22}^+$ ($\lambda = 10790$\r{A}), but the wavelength of the other DIBs do not correspond to the strong electronic transitions of ionized PAHs. However, as \citet{cox14} pointed out, the pure gas-phase spectra of ionized PAHs are required for the firm identification of NIR DIBs with ionized PAHs.

\section{Summary}

In order to search for new DIBs in the NIR wavelength range and study their properties, we obtained NIR high-resolution spectra of 25 early-type stars with color excesses of $0.07 < E(B-V) < 3.4$ using the newly developed NIR Echelle spectrograph WINERED. Consequently, we identified 15 new DIBs in the wavelength range $0.91 < \lambda < 1.32$ $\mu$m in addition to five DIBs previously detected in this wavelength range. For the first time, we investigated the correlations among NIR DIBs, eight strong optical DIBs investigated by \citet{fri11} ($\lambda \lambda$5487.7, 5705.1, 5780.5, 5797.1, 6196.0, 6204.5, 6283.8, and 6613.6), and the reddening of stars with a large number of lines of sight. Our findings are summarized as follows:

\begin{enumerate}

\item All identified NIR DIBs are found to have correlation coefficients with $E(B-V)$ that are not as high as those of the optical DIBs. The lower correlation coefficients of NIR DIBs with $E(B-V)$ show that the abundance of the NIR DIB carriers depends on some physical properties of gas clouds, such as UV flux, as well as on the amount of gas in the line of sight.

\item Three NIR DIBs, $\lambda \lambda 10780, 10792, \text{and } 11797$, are found to be well correlated with each other, suggesting that these three DIBs consist of a ``family,'' wherein the carrier molecules share similar physical and chemical properties. Because some data points do not quite fit the correlation, these DIBs would appear to originate from a different molecule.

\item The three strongest NIR DIBs, $\lambda \lambda 10780, 11797, \text{and }13175$, are found to be correlated better with $\lambda \lambda 5705.1, 5780.5, 6204.5, \text{and }6283.8$ ($r=0.8 - 0.9$) than with $\lambda \lambda 5797.1, 6196.0, \text{and }6613.6$ ($r=0.6-0.7$). Moreover, the NIR DIBs are found to be relatively weaker in $\zeta -$type clouds, where the molecules are shielded from UV flux, in the same manner as $\lambda 5780.5$, whose carrier is proposed to be a cation molecule with high ionization potential. Considering the similarity between the strongest NIR DIBs as well as some other NIR DIBs with $\lambda 5780.5$, we suggest that the carriers of these three NIR DIBs are also cation molecules.

\end{enumerate}

We are grateful to the staff of Koyama Astronomical Observatory for their support during our observation. We thank Alan T. Tokunaga and Setsuko Wada for their useful comments. We would like to acknowledge the helpful comments made by the anonymous referee. This study has been financially supported by KAKENHI (16684001) Grant-in-Aid for Young Scientists (A), KAKENHI (20340042) Grant-in-Aid for Scientific Research (B), KAKENHI (26287028) Grant-in-Aid for Scientific Research (B), KAKENHI (21840052) Grant-in-Aid for Young Scientists (Start-up), and the Japan Society for the Promotion of Science, MEXT-Supported Program for the Strategic Research Foundation at Private Universities, 2008-2012 (No.S0801061) and 2014-2018 (No. S1411028). S.H. is supported by Grant-in-Aid for JSPS Fellows Grant No. 13J10504.

redpajama_set_name: RedPajamaArXiv


WARREN, Mich., July 23, 2015 /PRNewswire/ -- Universal Truckload Services, Inc. (NASDAQ: UACL) today reported second quarter 2015 net income of $13.3 million, or $0.44 per basic and diluted share, on total operating revenues of $295.0 million. This compares to $13.6 million, or $0.45 per basic and diluted share, during second quarter 2014 on total operating revenues of $307.5 million.
Operating revenues from transportation services decreased $17.4 million, or 8.8%, to $180.1 million in the quarter ended June 27, 2015, due to a 6.8% year-over-year decrease in loads and a 2.8% decrease in average operating revenues per load, excluding fuel surcharges, compared to the quarter ended June 28, 2014. As previously communicated, second quarter 2015 operating revenues reflect lower demand, particularly in our steel, energy and other heavy haul operations, but a generally more stable volume and pricing environment for truckload transportation services compared to earlier 2015.
Value-added services revenues decreased $0.9 million in the most recent quarter, due to fewer operating locations compared to the comparable period last year. Revenues from intermodal services increased 17.1%, to $39.8 million from $34.0 million in the second quarter of 2014. The $5.8 million net increase in revenues from intermodal services includes a $5.9 million, or 19.2% increase in our intermodal drayage services, which is benefiting from increased import activity, capacity shifted from other businesses, and a 12.6% increase in average operating revenues per loaded mile, excluding fuel surcharges.
Consolidated income from operations decreased 6.1% to $22.9 million, compared to $24.4 million in second quarter 2014. EBITDA decreased 1.9% to $31.8 million in second quarter 2015, compared to $32.4 million one year earlier. Our operating margin and EBITDA margin for second quarter 2015 are 7.8% and 10.8% of operating revenues. These profitability metrics compare to 7.9% and 10.5%, respectively, in second quarter 2014. Consolidated income from operations in the quarter ended June 27, 2015 also reflects a $1.2 million decrease in selling, general and administrative expenses, which are partially offset by a $0.8 million increase in depreciation and amortization expense.
Income from operations in our transportation segment decreased $0.6 million, or 6.1%, to $9.2 million in second quarter 2015 from $9.8 million one year ago, due to a $6.7 million decline in transportation segment revenues. Income from operations in our logistics segment decreased $3.4 million, or 21.1%, to $12.7 million from $16.1 million in the comparable 2014 quarter. Logistics segment income, which originates from Universal's value-added services and dedicated transportation operations, is lower in second quarter 2015 compared to a year earlier primarily due to changes in the number of operating locations. Logistics segment revenue in second quarter 2015 declined 5.2% or $5.9 million, reflecting the impact of customer-dedicated facilities we closed in second quarter 2014 among other factors.
Universal's Chief Executive Officer, Jeff Rogers, observed, "Demand for our transportation and logistics services met our recent expectations, reflecting continuing weakness in truckload volumes, but steady volumes and firm pricing in other businesses. We are especially pleased with the continuing strength of our intermodal business, which is prospering due to drayage operations benefiting from increased international trade. Our value-added services also achieved anticipated revenues and margins in the second quarter, as we began the launch of a large value-added project which will positively impact financial results later this year.
"Universal's recent tender offer reduced the number of Universal shares outstanding by about 5.3%, returning capital not needed to support our asset-light business model to our shareholders and enhancing future EPS. Our commercial focus remains driver development, extending relationships with existing customers, and new customer acquisition. These strategies will drive the growth of our intermodal, brokerage and logistics businesses and, we believe, improve the value of our truckload and dedicated transportation services businesses as well."
Universal calculates and reports selected financial metrics in connection with lending arrangements, or to isolate and exclude the impact of non-operating expenses related to our corporate development activities. These statistics are described in more detail below in the section captioned "Non-GAAP Financial Measures."
As of June 27, 2015, we held cash and cash equivalents totaling $7.7 million and marketable securities totaling $15.1 million. Outstanding debt totaled $221.6 million and obligations pursuant to capital leases were valued at $2.5 million. Capital expenditures in second quarter 2015 totaled $7.0 million.
Universal Truckload Services, Inc. also announced today that our Board of Directors has declared a quarterly cash dividend of $0.07 per share of common stock. The dividend is payable to shareholders of record at the close of business on August 3, 2015 and is expected to be paid on August 13, 2015.
We invite analysts and investors to participate in our quarterly financial performance conference call, during which Jeff Rogers and David Crittenden, CFO, will discuss Universal's second quarter 2015 financial performance, the demand outlook in our key markets, trends impacting our business, and the outcome of our modified "Dutch auction" tender offer, which expired on July 8, 2015.
A replay of the conference will be available beginning two hours after the call through August 21, 2015, by calling (855) 859-2056 (toll free) or +1 (404) 537-3406 (toll) and using conference ID 74274014. The call will also be available on investors.goutsi.com.
Universal Truckload Services, Inc. is a leading asset-light provider of customized transportation and logistics solutions throughout the United States, and in Mexico, Canada and Colombia. We provide our customers with supply chain solutions that can be scaled to meet their changing demands and volumes. We offer our customers a broad array of services across their entire supply chain, including transportation, intermodal, and value-added services.
Excludes operating data from Universal Logistics Solutions International, Inc., in order to improve the relevance of the statistical data related to our brokerage services and improve the comparability to our peer companies. Also excludes final mile delivery and shuttle service loads.
Average length of haul is computed using loaded miles, excluding final mile delivery and shuttle service loads.
Excludes storage yards, terminals and office facilities.
In addition to providing consolidated financial statements based on generally accepted accounting principles in the United States of America (GAAP), we are providing additional financial measures that are not required by or prepared in accordance with GAAP (non-GAAP). We present EBITDA as supplemental measures of our performance. We define EBITDA as net income plus (i) interest expense, net, (ii) provision for income taxes and (iii) depreciation and amortization, and less other non-operating income, or EBITDA. You are encouraged to evaluate these adjustments and the reasons we consider them appropriate for supplemental analysis.
(a) EBITDA margin is computed by dividing EBITDA by total operating revenues for each of the periods indicated.
We present EBITDA because we believe it assists investors and analysts in comparing our performance across reporting periods on a consistent basis by excluding items that we do not believe are indicative of our core operating performance.
Because of these limitations, EBITDA should not be considered in isolation or as a substitute for performance measures calculated in accordance with GAAP. We compensate for these limitations by relying primarily on our GAAP results and EBITDA only supplementally.
SOURCE Universal Truckload Services, Inc.


text:
Donnell DE-56
Donnell
Earl Roe Donnell, Jr., born 3 September 1918 in Temple, Tex., enlisted in the Naval Reserve 24 August 1940 and was appointed an aviation cadet 6 December. Ensign Donnell was killed in action while serving in Scouting Squadron 6 on board Enterprise (CV-6) during the attack on the Marshalls 1 February 1942. For his courage in pressing home his attack in the face of enemy fighter opposition and heavy antiaircraft fire, he was posthumously awarded the Air Medal.
(DE-56: dp. 1,400, 1. 306', b. 37'; dr. 9'5" B. 24 k.; cpl. 186; a. 3 3", 3 21" tt. 8 dcp., 1 dcp.(hh.) 2 dct.; cl. Buckley )
Donnell (DE-56) was launched 13 March 1943 by Bethlehem Steel Co., Hingham, Mass.; sponsored by Mrs. E. R. Donnell, mother of Ensign Donnell; and commissioned 26 June 1943, Lieutenant Commander F. C. Billings, USNR., in command.
Donnell sailed from Boston 31 August 1943 for transatlantic convoy duty. She guarded the safe passage of four convoys to Londonderry and return in the buildup for the invasion of Europe in June. At sea bound for Londonderry again on her fifth voyage, on 3 May 1944 Donnell made a sound contact, then sighted a periscope a few minutes later and pressed home a depth charge attack. Simultaneously she was struck by a torpedo which blew off her stern. Explosion of her own depth charges inflicted additional damage on the escort. Her casualties were 29 killed and 25 wounded.
Donnell was towed by Reeves (DE-156), Hopping (DE-155), and HMS Samsonia to Dunnstaffnage Bay, Scotland, arriving 12 May. Since repairs would have involved extensive reconstruction, she was placed in commission in reserve at Lisahally, Northern Ireland 20 June 1944, for use as an accommodation ship. She was reclassified IX 182, 15 July 1944. Towed to Plymouth, England, in July to embark passengers and take on cargo, Donnell was towed in August to Cherbourg, France, where she supplied electric power to shore installations. In February 194.5 she was returned to England, and served as barracks ship at Portland and Plymouth until towed back to the States, arriving at Philadelphia Navy Yard 18 July 1945. She was decommissioned 23 October 1945, and sold 29 April 1946.


text:
Driving a Filthy Car in Makati is Illegal, and Other Violations
It's cheaper to get your car washed than to get fined.
By Mario Alvaro Limos | Apr 17, 2019
When it comes to law enforcement, Makati's finest are reputed to be obstinate and unbending toward violators. That's why when Makati passes a new ordinance, everyone pays attention.
One such ordinance is that public utility drivers are prohibited from wearing sando and slippers. The ordinance helps professionalize those in the PUV industry, which includes jeepney drivers, bus drivers, taxi drivers, and Grab drivers.
While prohibiting the wearing of sandos is more concerned with upholding decorum and professionalism, banning the use of slippers is more about safety, as slippers are loose and tend to latch on the pedals and floor mat.
Such ordinances are laudable, but others are open to interpretation.
For example: "Arrogant – P150"
What is arrogance? It could be open to interpretation, especially by enforcers who are questioned by drivers about why they are being flagged. In 2011, over 400 people were fined for being arrogant.
Here are other interesting violations and fines you should be aware of in Makati.
Operating a Habal-habal: P5,000
Habal-habal are colorum motorcycles that offer a quick ride to your destination. They are cheap, quick, and illegal. For as little as P100, a rider can weave in and out of traffic from EDSA-Ayala to any point in Makati, Ortigas, or Taguig in less than 10 minutes. It is like Angkas, but unregistered, and hence, illegal.
Urinating, Defecating, and Spitting: P100
Perhaps another zero should be added to the fine for urinating, defecating, and spitting in public spaces, especially since urinating and spitting is rampant at bus stops and MRT stops in the city. Blech.
Jaywalking: P200
For jaywalking, P200 seems like a cheap price to pay for endangering the lives of motorists and pedestrians. If lawmakers are pushing for capital punishment to deter those who commit heinous crimes, why not raise the penalties and fines to deter jaywalkers? If no fine can be paid, a 30-minute detention also works.
Dirty Vehicles: P300
Now you have a reason to send your car to the car wash. It is more expensive to incur a fine for driving a dirty car than having it cleaned. Unsanitary or unclean vehicles are illegal on Makati streets. Enforcers are also concerned about your car's plates, so make sure to have those cleaned, too. In 2011, over 100 people were apprehended for driving filthy cars.
Littering, Illegal Dumping of Garbage: P500
Makati's central business district is one of the cleanest in the country because of this particular ordinance. Solid waste management remains a serious challenge for many of Metro Manila's residents who transit through Makati every day. Increasing the teeth on this ordinance should be reconsidered.
Illegally Counter-flowing, Violating No-entry Sign: P2,000
Salcedo Village and Legaspi Village, the two residential-commercial villages on either side of Ayala Avenue, have confusing one-way streets. These two villages are also the heart of Makati's CBD, so enforcement is extra strict here. Save yourself from being fined P2,000 by being aware of road flow and no entry signs.
Using Cellphone While Driving: P250
Distracted driving does not seem to be a very serious offense, as it fetches a fine of only P250, less than driving a dirty car, but much more dangerous.
Makati Ordinances
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