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Category Archives: Fiction Reviews
The Urban Fantasy Anthology – Review
Review of The Urban Fantasy Anthology. Ed. Peter S. Beagle and Joe R. Lansdale. San Francisco: Tachyon, 2011. $15.95.
In The Urban Fantasy Anthology, Peter S. Beagle and Joe R. Lansdale have created a much-needed collection of urban fantasy suitable for classroom instructors, academics, and interested laypersons alike. As Beagle notes in his introduction, "urban fantasy has become so vibrant, and has evolved so rapidly, that it has emerged as a distinct marketing category." This book brings together a variety of important stories in the field from both grand masters of fiction and comparative newcomers, creating an important text for anyone interested in urban fantasy. Perhaps more importantly, however, the anthology creates a collection that leaves the impression of a genre (and series of sub-genres) still developing.
Beagle and Lansdale have chosen to divide the collection into three categories: Mythic Fiction, Paranormal Romance, and Noir Fantasy. The sections are introduced by Charles de Lint , Paula Guran, and Joe R. Lansdale, respectively. However, the section introductions illustrate the difficulties inherent in defining a genre, particularly one as new as urban fantasy. Indeed, beyond the basic element of the fantastic in a modern setting, the various section editors themselves show little consensus about what constitutes an "urban fantasy" story. In the introduction, Beagle claims that "I still think that urban fantasy's most important distinction is that it isn't The Lord of the Rings" (9). Each section editor's introduction provides his or her ideas about the concept of "urban fantasy," deepening and enriching the conversation surrounding the genre and its various sub-genres—a move that will, I suspect, more firmly entrench the various categories, despite everyone's apparent reluctance to do just that.
Charles de Lint entitles his section introduction "A Personal Journey into Mythic Fiction"—and given the fact that de Lint's novel The Jack of Kinrowan: A Novel of Urban Faerie inspired the term "urban fantasy" (much as his fiction participated in inspiring the genre itself), the development of the genre and de Lint's development as an author might well be synonymous. However, de Lint writes that he "found the terms 'urban fantasy' and 'contemporary fantasy' unsatisfactory . . . partly because not all the works we were looking at were urban, or set in the present day" (18). His use of the term "mythic fiction," then, arises out of the fact that, as he notes, the difference between other urban fantasy books and what he calls mythic fiction is that "the magical/mythic/folkloric elements of these books is colour and shade, rather than the substance of the story. The new urban fantasy story remains rooted in the genres from which it sprang. Its magic is more often matter-of-fact—bricks and mortar—rather than something that leaves the reader with a sense of wonder." Mythic fiction, he implies, should create that wonder missing in other kinds of urban fantasy.
Included in the first section are two stories by de Lint himself, as well as one each by Emma Bull, Neil Gaiman, Jeffrey Ford, and Peter Beagle. These are certainly not stories of the matter-of-fact or brick and mortar, but their forays into the mythic vary widely. Gaiman's otherwise apparently prosaic tale of a novelist-turned-screenwriter invokes the magic of the silver screen in the era of silent film as well as that of Victorian stage magicians, while Beagle's story of a medieval tapestry unicorn set free in the modern world by a sympathetic museum-goer reads more like the works included in the "Paranormal Romance" section. All of the stories, however, deal with worlds of myth and legend, from a road-tripping Jesus and Satan in Ford's "On the Road to New Egypt," to an elf who plays music in a coffee shop in de Lint's "Make a Joyful Noise," to a Native American shape-shifting crow in Bull's "The Bird that Whistles."
Like the other section editors, Guran is uncomfortable with the term "urban fantasy"—but unlike de Lint and Lansdale, she also takes exception to the term "paranormal romance," noting that many of the works categorized as paranormal romance are as likely to trace their origins to other genres. As she points out, Charlain Harris's initial Southern Vampire Mysteries novel (the basis for the HBO series True Blood) "won an Anthony Award as Best Paperback Mystery of 2001" (139, emphasis Guran's). For Guran, the central shared characteristic of fiction in this category is "an intersection of 'the other'—the magical, the strange, the weird, the wondrous, the dark that illumines, the revelation of the hidden—with the mundane, the world we know" (145).
The anthology includes in this section stories by de Lint, Kelley Armstrong, Norman Partridge, Carrie Vaughn, Patricia Briggs, Bruce McAllister, Suzy McKee Charnas, and Francesca Lia Block. In many ways, Guran is right—Block's story of a grieving-mother-turned-zombie-hunter-P.I. ("Farewell, My Zombie") and Vaughn's tale of a party-crashing zombie created by a controlling boyfriend ("Kitty's Zombie New Year") seem more mystery than romance. Similarly, Charnas' "Boobs"—the story of an adolescent girl becoming a werewolf—ends more in horror than romance (though not entirely in either), as does Armstrong's "A Haunted House of Her Own." Indeed, of all of the excellent offerings in this section, only McAllister's "Seeing Eye" seems to conclude with the potential for love that is the hallmark of commercial fiction romance novels.
Although none of the authors of the introductions are entirely at ease with the term "urban fantasy," Lansdale is the most outspoken: "It's not my purpose here to round up these stories and brand them. They can be tagged to some degree, but they are not confined by the tag" (275). Lansdale also notes that "this section of stories owes less to Buffy the Vampire Slayer and more to noir and writers who tripped the dark fantastic with gleeful enthusiasm" (276) such as Raymond Chandler, Dashiell Hammett, Ernest Hemingway, Richard Matheson, Ray Bradbury, Harlan Ellison, and Flannery O'Connor (among others).
The Noir Fantasy section includes two stories by Lansdale and one each by Thomas Disch, Susan Palwick, Holly Black, Tim Powers, and Al Sarrantonio. Steven R. Boyett's short story "Talking Back to the Moon," also included in this section, is the only previously unpublished work in the collection. Only in this portion of the anthology do the selections seem to fully live up to their section name: these stories are dark. Disch's "The White Man" is chilling in its depiction of a young Malawi girl encouraged to hunt vampires in Minnesota, and in Palwick's "Gestella," the reader follows a domesticated werewolf wife as she spirals down to her inevitable horrific end. Black's "The Coldest Girl in Coldtown" dispels any romantic notions about vampirism, while "Talking Back to the Moon" offers a bleak post-apocalyptic world, even for werewolves and centaurs. "The Bible Repairman" and "Father Dear" both feature parents making dreadful sacrifices for their children.
The anthology has a few weaknesses, perhaps unsurprisingly for a collection attempting, in part, to both stabilize and expand conceptions about a relatively new genre. Guran's section introduction, for example, relies fairly heavily upon comments in Landsdale's section introduction, though Guran's precedes Lansdale's—but this is really only a problem for a reader reading the anthology in strict order, and I suspect that most casual readers will pick and choose among the stories available. More problematically, Beagle's introduction attributes "cheerful werewolf heroines running radio call-in shows" to Laurel K. Hamilton's Anita Blake series (10)—a mistake that perhaps indicates an only passing familiarity with the "Paranormal Romance" version of urban fantasy, as the werewolf in question is actually from Carrie Vaughn's Kitty Norville series. Ultimately, though, The Urban Fantasy Anthology offers a much-needed collection of what Beagle calls "raw, consciously commercial fiction, feeding an unquenchable hunger for walks on the wild side, blending and shaking up familiar themes until they are transformed into something new and meaningful" (11)—an affordable collection that brings together some of the best stories to be found in urban fantasy, accompanied by an accessible critical framework. Despite its minor flaws, it's an absorbing collection—so much so that I read it in a single sitting—and the consistently well chosen stories overcome the taxonomical tensions among the various section introductions.
~Margo Bond Collins
* Originally published in Monsters and the Monstrous. 2.1 (2012): 96-8. (http://monstersjournal.net/)
1 Comment Posted in Fiction Reviews Tagged fiction, reviews, urban fantasy


Added by Les van P.
A group of casual tennis players for evenings, Saturday mornings, or whenever the weather is good. The purpose is to bring people together so they can play. Join this group if you are looking for tennis opponents or doubles teammates.


FeetUp Yoga DEMO with Ali Monteiro- Try it!
Turn your world upside down with the FeetUp Trainer.
Come and find out more about this fantastic inversion assistant.
Master safe inversions without pressure on the neck and spine.
I will lead you through an exciting class where you will learn to use the FeetUp Trainer.
The FeetUp Trainer will help take pressure from the back, shoulders, and wrists. It helps to deepen twists and hip openers while supporting the back.
So many fun posses and beautiful flows.
What is an inversion and what are the benefits?
An Inversion is an asana in which your head is below your heart.
Reversing the blood flow improves circulation.
Increases oxygen and blood to the brain for clearer thoughts, better concentration and calms the nervous system.
Activates the lymph, strengthening the immune system and preventing illness.


Today, I'd like to say thank you for using your talents to inspire others and bring joy to those in need! I always knew that sewing people were the most generous bunch, but it's a great reminder to see those finished NICU charity smocks arriving on my doorstep day after day. So, thank you!
If you'd like to join the NICU charity sew along, there's still time! You can find all the info here and join the Facebook group here.
Today I'd like to offer a big thank you giveaway to my readers and friends sewing along with us in the NICU sew along.
Enter for your chance to win a yard each of these new (not yet in stores!) Ann Kelle Urban Zoologie Minis fabric in three designs, which would be perfect for your next charity sewing project. These were generously donated by the designer herself as a way to say thank you for everything you do.
Good luck, sewing friends, and keep on using your love of sewing to bring joy to the world around you! Giveaway open worldwide through 9/19.
These tiny prints are adorable -- perfect for little smocks! Love them.
How awesome is this??!! Love these fabrics! Thank you for the chance to win!!
I am thankful for my family on 9/11 and the freedoms that America affords them. Sewing along on the NICU Smocks for Charity.
Thank you for the chance to win these adorable prints!
I'm grateful for my family today. I would love to use these fabrics in baby quilts for my local NICU. Thank you!
I am thankful for my family today. Hold your family close and cherish every moment and memory with them.
Thank you for this great giveaway! I work at a hospital with an 80 bed NICU and would love to use this fabric to stitch up some smocks for them!
I am thankful for my husband and my 2 sons; they make my life so wonderful!
I am so thankful for my family. Enjoy every minute. Thank you for the chance to win.
I am thankful for having the opportunity to sew today. Thank you also for the chance to win. These would be great for making the smocks.
Very sweet fabrics. I am thankful that the sun is shining and that I will be able to spend time in my sewing room today.
I am thankful to get up each and every day, my family's health, food on the table, a beautiful home and of course a super fantastic family! This fabric is adorable and would be perfect to make something for my new grandnephew!
thankful for good friends and a lunch date!
I have 10 on the way to you!
Super cute fabrics!! I'm thankful for so many things. My sister just came through back surgery with flying colors and my son who is serving in the USMC is home safe.
I'm grateful for my family and the nice weather today!
I am grateful for my loving and faithful husband, and our two grown children. He is retired Army, and for most of the day on 9/11, I did not know that he was safe. So very thankful that he WAS kept safe!
I am thankful for my family and Jesus.
I am thankful for family and friends today and everyday.
Love the fabrics. Thanks for a chance to win. Thankful for so much in my life everyday, but today I'll give a special shoutout to my grandbabies. There is no love like it.
So cute. Thanks for the giveaway.
I'm thankful for the upcoming fall season. It actually feels like fall today and I'm so excited for pumpkins and crunchy leaves and Christmas gift sewing!!
I am thankful for my wonderful family.
I am thankful for the much cooler weather and the ability to enjoy it. Also thankful for family and good health!
I am grateful to my hubby - as always, but especially now. I recently went through a thumb reconstruction and he has had to do everything for me. He has even offered to cut fabric for me when I transition back into sewing!
I just got an email from a friend telling me her husband has cancer.
So today I am especially thankful that my husband and kids are healthy.
I'm thankful for generous people in the world. Generous with their time, talents and resources!
where do I find the pattern for the charity smocks?
I am thankful for my family today.
I have just discovered you via Ann Kelle and love her fabrics! With a friend heartbroken as she struggles to get her daughter to eat enough each day, I am grateful that I have happy healthy children and a happy home.
I have a wonderful husband and 2 great children, 3 grandchildren. All is right in the world.
I am thankful for my healthy grandkids.
I am thankful for my husband. Thank you for all you do, and the giveaway.
Thankful for time with my husband today and forego us weather.
So cute. Our guild collected nearly 100 quilts for charities this summer. I made 5. These fabrics would be so fun to sew with.
I am very thankful for my loving husband!! He is a gem!
I am thankful for my family.
Holly D...also sorry if this shows up 3x. Having troubles leaving a comment.
I am most thankful for my family!!
I am so thankful for the salvation I have through Jesus Christ - every other blessing takes second place, but I am also SO thankful to have a dishwasher again - ours has been broken since February! Today we had a new one installed ... yeah!
I am very thankful for my family, especially my one and only grandchild. Thanks for the opportunity to win some fabric, I am working on my smocks and can use it to make more.
I'm thankful for five healthy kids, and five healthy grandkids! And I'd definitely like to sew some itty bitty loving for the NICU babies in our area--Denver. There is so much joy in making something that will be used and cherished... and bring some smiles for (maybe a bit stressed-out) families of these tiny gifts of love).
I'm thankful for the blue skies and sunshine!!
Today I am thankful for cooler weather!
Those animal prints are adorable!
Beautiful fabrics. I am thankful today for being able to finish my jobs in the kitchen so I can have more time for ms family in the weekend. Thank you for the chance to win!
I am thankful that my family is safe.
Nice looking fabrics. I am so thankful for all of my family and grandchildren. Thank you for the opportunity to win.
Thankful for my spunky 2 year old who amazes me every day.
I'm thankful that my husband and I got to spend the day with my youngest who lives in Iowa driving to Tulsa from Texas to visit with my oldest in Oklahoma. It is his 30th birthday and we surprised him at the high school where he is the chaplain. A wonderful day!!
I'm thankful for my new nameless nephew!
So many blessings and things to be thankful for in my life! One thing: family & friends who I love.
I'm thankful for Jesus, my husband, my kids and my community.
I am thankful for my family - I love them so much. And I am thankful for the ability to sew.
I'm thankful for the many blessings in my life; Family, love, health.
And I love the fabrics! Ducks, cats and Frenchies!
I'm thankful for the women's ministry at my church. We are about to begin the Beth Moore Simulcast in just a few hours. It's been fun planning and preparing for this day with sisters in Christ.
I am so thankful for many things in life we take for granted. I am thankful for talented people like you who share your gift and inspire others.
Thankful for beautiful fall weather and great family to enjoy it with :).
I am thankful for my husband and two sons.
I'm thankful for my wonderful famliy :) Thanks so much for this great giveaway!
Good morning....I'm thankful for my new baby - 3 weeks old tomorrow and the sweetest baby ever!
Thankful that my son and daughter-in-law are foster parents-to-be and able to love, cherish and care for anothers child when they can not.
Beautiful fabric! Thanks for the chance to win!
I am grateful for my husband and our wonderful family. Healthy daughters and 5 healthy grandchildren.
Thankyou for the chance to win. I am grateful for all the blessings God has given me, especially the ones I didn't know were blessings.
I am thankful to have a sewing machine that works.
I'm thankful for my little granddaughter.
I am thankful for my faith!
I'm thankful we recently sold my mom's house. 2 1/2 years after her death and a lot of hard work on it.


text:
using System.Threading.Tasks;

namespace TestData.Async.AsyncMethodNamesShouldBeSuffixedWithAsync.CodeFixProvider
{
    public class AsyncGenericTaskMethodWithoutAsyncSuffix
    {
        public async Task<int> AsyncGenericTaskMethodAsync()
        {
            return 1;
        }
    }
}

redpajama_set_name: RedPajamaGithub


text:
The Venetian Hills - Renaissance art in the foothills of the Dolomites
Ravishingly beautiful landscapes from vine-clad foothills to the peaks of the Dolomites.
Altarpieces and frescoes by Venetian masters, mediaeval to Rococo.
Some of the loveliest hill towns in Italy, including the birthplace of Titian.
Option to combine this tour with Friuli-Venezia Giulia, 7–12 October 2019.
03 - 07 Oct 2019 £1,880 Book this tour
The Dolomites and the Cadora Valley, wood engraving 1893 after John McWhirter.
Expert lecturer
'Hills' and 'Venice' are not accustomed to finding themselves in the same sentence; sited on (and sometimes under) an estuarial lagoon, elevation above (or below) sea level in Venice is measured in centimetres. But on a clear day a range of hills can be seen rising to the north. On a very clear day the snowy peaks of the Dolomites come into view.
Towards the end of the Middle Ages the proud little communities which populated these hills one by one submitted to the rule of La Serenissima, as did much of northern Italy. Political hegemony was followed by cultural influence, clearly manifested still in the disorientating sight of Venetian-style Renaissance palazzi set against precipitous pine-clad hillsides.
But the cultural forces did not flow only in one direction. As is often the case with an artistically flourishing metropolis, many of the creators were outsiders. Titian was born in the rugged Cadore mountains, Cima from the gentler hillside town of Conegliano, Marco Ricci from hilltop Belluno. These and many other artists enjoyed successful careers in Venice, but most kept in contact with their natal towns, accepting commissions for, or donating paintings to, their parish church.
These hill towns are among the loveliest in Italy, and they are set in ravishing landscapes which range from vine-clad foothills to soaring limestone peaks. Most of them are quite small, but the architectural ambitions of their inhabitants were otherwise: the historic centres are dense with fine buildings and arcaded streets which give protection from mountain downpours and summer sun.
The ostensible theme of this tour is painting of the fifteenth and sixteenth centuries, but other aspects of the art and history of the region will not be ignored. The base is Follina, a tiny community which grew up around a monastery in the mountains.
Fly at c. 1.00pm (British Airways) from London Gatwick to Venice. Drive through the hills to Follina where all four nights are spent.
Vittorio Veneto, Conegliano. The tiny city of Serravalle (now joined with Cèneda to form Vittorio Veneto), occupying a gorge scoured by the River Meschio, has a fine group of mediaeval and Renaissance buildings, 15th-century frescoes in the chapel of S. Lorenzo and a Titian in the cathedral. In the church of Santa Maria in Cèneda there is an exquisite Annunciation by Previtali. Drive to the birthplace of Giambattista Cima del Conegliano, the lovely town from which the artist took his name, that spreads down a hillside below the remains of a castle. Visit Cima's house and the cathedral to see one of his greatest works (1492).
Pieve di Cadore, Belluno. Titian was born in the little town of Pieve di Cadore; see here the family home and the parish church with paintings by Titian and family. In the afternoon drive north along the valley of the Piave into an ever more dramatic mountain landscape. Sitting athwart a promontory looped by the Piave, Belluno is a beautiful little city with a Renaissance cathedral and Venetian-style palaces. Among the fine paintings is an exquisite Madonna & Child by Cima in the Museo Civico.
Bassano, Feltre. Bassano del Grappa is a highly attractive town in the foothills of the Dolomites with a series of picturesque squares with painted façades. Home of the prolific Bassano family of painters, there are several of their works in the civic museum. Stacked up along the ridge of a hill, Feltre is another architectural outpost of Venice with striking buildings in various styles. See the Rizzarda collection of early 20th-century arts and crafts and the 1802 theatre in the town hall.
San Fior, Treviso. Descend to San Fior, a little town on the densely populated plain at the foot of the hills. Riven by canals and streams, San Fior has an altarpiece by Cima. Once an important fortress city, Treviso has a fine historic centre with imposing public buildings and many painted façades. Selective visits here include the extraordinary frescoes of learned monks in the chapter house of St Nicholas by 14th-cent. painter Tommaso da Modena. Fly from Venice airport, arriving at Gatwick c. 7.00pm.
If combining this tour with Friuli-Venezia Giulia: there is a refreshment break at Venice airport before the coach continues to Udine.
Dr Carlo Corsato
Dr Carlo Corsato. Art historian and lecturer specialising in early-modern art and architecture in Italy and Flanders. He obtained his PhD from the University of Verona on 16th-century painting in Venice and the Veneto. He has lectured and given invited talks at a number of institutions, including the Morley College, the Courtauld Institute, and the universities of St Andrews, Glasgow, and Buckingham. He was visiting scholar at the Dutch Institute in Florence and St John's College, Cambridge. He has contributed to international scholarly journals and exhibition catalogues, and co-edited the first completed monograph on the church of Frari, Venice.
The Venetian Hills and Friuli-Venezia Giulia combined
Flights (Euro Traveller) with British Airways (Airbus A319); travel by private coach; breakfasts; 1 lunch and 3 dinners with wine, water, coffee; all admissions; all tips for waiters, drivers; all taxes; the services of the lecturer.
Hotel dei Chiostri: a 4-star hotel in the little hill town of Follina, installed in former abbey buildings.
The tour involves quite a lot of walking, some of which is uphill or in the town centres where vehicular access is restricted. Streets are often cobbled, and the tour should not be attempted by anyone who has difficulty with everyday walking and stair-climbing. Most days involve a fair amount of driving. Average distance by coach per day: 62 miles.
'Once again a very pleasant holiday – one comes home very pleased with the overall experience.'
'The historic centres of the hill towns provided one treat after another in location we would not otherwise have accessed.'
'The lecturer was absolutely first class in every way.'
'The lecturer's humour and relaxed manner, his beautifully clear enunciation and passion and knowledge of Titan and the other medieval and renaissance painters made it a real pleasure to absorb so much history, politics and art and architectural knowledge.'
Friuli-Venezia Giulia The border lands of northeast Italy
03 - 07 Oct 2019 MF774
Expert lecturer: Dr Carlo Corsato
The Cathedrals of England Ely, Lincoln, Durham, York, Coventry, Gloucester, Bristol, Wells, Salisbury, Winchester
30 Sep - 08 Oct 2020 £2,840
The London Backstreet Walk From Hyde Park to The Tower
Art in Madrid The Great Galleries
04 - 08 Nov 2020 £1,980
Medieval Alsace Both sides of the Rhine in France & Germany

redpajama_set_name: RedPajamaCommonCrawl


Job postings by social-impact employers often come with a big list of must-have skills. After all, these employers are looking for people who can solve some pretty tough challenges.
But other than soft skills, what kind of experience and technical expertise will get you noticed by social-impact employers?
This is probably one of the top criteria on a hiring manager's checklist.
How can you show this experience?
Have you worked on a related project as part of your college coursework or as a leader of a student organization? In other professional roles? In an internship? Through volunteer work?
If you answered no to all of the above, what can you do to obtain this experience?
If you are a student, you may be able to design your own internship at an organization of interest to gain experience on relevant projects. Some colleges have internship funding that you can apply for and pitch an internship idea to your dream organization.
Even if your college does not have internship funding, you may still be able to pitch an internship idea to staff working on projects in your interest area. If you don't ask, your chances are zero. And if you do ask, your chances can only go up from there.
You may also be able to volunteer at an organization working on project areas of interest. Idealist.org is a great place to look for volunteer opportunities.
Many jobs require specific technical skills. Look at multiple job postings that interest you and see if certain technical, analytical, language, or computer skills are needed.
Do you have a relevant degree or certification? Can you list specific technical coursework and computer software skills that are relevant to the job? Do you speak more than one language?
If needed, pursue relevant certificate programs or consider graduate programs in nonprofit management. Take online computer software courses or check for courses with local colleges, libraries, or community education departments. Conduct informational interviews to get the best advice on where to obtain these technical skills and make sure to ask which ones are required, and which should fall further down your list of priorities.
The best staff are problem-solvers. They have the ability to think creatively and solve problems in innovative ways. Obstacles do not stop them and they get work done.
Have you taken the initiative to make a process more efficient? Ever save an organization time or money? Solve a problem that seems unsolvable? Reach a consensus on a challenging issue that looked like it would end in a stalemate?
Find successful frameworks for creative problem solving. Practice by doing. Seek out small-scale challenges to take on. Use a creative problem solving framework to solve these challenges. Interview people that you view as creative problem solvers and ask them what approach they take.
Management skills can encompass a lot of different skill areas: ability to develop a vision for an organization or program, people management, project and budget management, time management, and fundraising skills. And don't underestimate soft skills. You may not need all of these in your professional tool belt but if you aspire to a manager or director role, they all play a part.
Have you ever developed a project and managed it from beginning to end? Did you manage a budget or raise funds? Have you juggled multiple projects? Ever adapt to a major change in plans?
Volunteer to manage or lead a project and you will gain many of these skills. Consider taking online courses in project management, people management, etc. If needed, explore relevant certificate program or consider graduate programs in nonprofit management.
You can be confident that hiring managers at many social-impact organizations will be scanning your resume for these four critical experiences and skills. Use the "How Can You Show This Experience" sections to help you design resume bullet content to show these skills.
Are there other key experiences or skills that social impact employers value? Do you work for a social-impact employer?
We would love to hear how you use any of these four experiences and skills in your work. Or let us know your ideas for how to obtain them. Share your thoughts in the comments below.


text:
No joke: Rival hockey teams finish game with a punch line
The Best Western in Canton, N.Y., could be a swinging kind of place Friday night ... and not because of the musical entertainment in the lobby.
That's where the Union and Rensselaer Polytechnic Institute men's hockey teams reportedly are both scheduled to stay on road trips less than a week after their Mayor's Cup game ended in a nasty skirmish that saw the head coaches go after each other on the ice Saturday in Albany.
Two players from each team will be suspended for their contests on Friday as the result of game disqualifications tacked on to five-minute majors, the big offenses among 125 minutes of penalties doled out after the final horn.
With 1.7 seconds left in the 2-1 victory, RPI players were ready to jump off the bench to celebrate snapping a 10-game losing streak to the Dutchmen. The horn sounded after a faceoff, but suddenly the 7,000 fans at Times Union Center were treated to pushing and name-calling that quickly escalated after Union players were caught up in the RPI swarm.
Union coach Rick Bennett and Engineers counterpart Seth Appert approached each other and were ready to rumble before the proverbial cooler heads (game officials and players) prevailed.
"I'm embarrassed about my actions," Bennett told The Times Union in the course of doling out apologies to just about everyone imaginable.
Appert was also decidely more gentlemanly once eveyone had time to reflect. "I have nothing but respect for Rick Bennett," he said. "He's a great coach and a great man."
OK, that's what they're saying now. But we have evidence that strongly suggests mixed feelings at best a few minutes earlier:


Whether dining at a standard pizza chain or Michelin-starred gastro pub, you can be sure that a large portion of adjectives and complex terminology will be on the menu.
Even the most experienced foodie has been caught out by a humble steak dressed up as 'Frenched chateaubriand à point on crushed heritage carrot', and many restaurant menus result in us feeling like we've wandered onto the final of MasterChef. Are these overly-descriptive paragraphs about our food's origin, quality, pedigree, favourite music, political leanings… really all that necessary?
This burgeoning trend is partly a consequence of modern cuisine being continually influenced by countless other cultures, which is surely a good thing. Much terminology used by chefs today is unusual to us due to its cultural roots – who honestly knows the difference between a burrito, tostada and chimichanga? Or maki, nigiri and iso sushi? Of course, many culinary terms still used today are French (France being the undisputed pioneer of gourmet cooking). In this case, deciphering what exactly you'll be served upon ordering a 'confit of duck with legumes émincé' is more an exercise in translation.
However, we can't help but feel that the gastronomes of today are taking food description a little too far – it seems as though nothing leaves a kitchen without being 'deconstructed', 'reduced', 'enhanced', or whipped into a 'foam'. As an antidote to the confusion and embarrassing mis-orderings that ensue from complicated food terminology, we've put together the ultimate 'Menu Cheat Sheet', designed to guide you through the culinary quagmire of semantics and adjectives, so you can be sure what'll end up on your plate. You're welcome!


UK: The Global Cement and Concrete Association (GCCA) has held its inaugural annual general meeting and symposium in London. Member companies ratified key deliverables for the association and set-out its priorities and work program. Albert Manifold, chief executive officer (CEO) of CRH, was confirmed as GCCA President and will serve for two years. Fernando A González, CEO of Cemex and Jianglin Cao, CEO of CNBM, were confirmed as Vice-Presidents.
The work program will focus on: position concrete as the sustainable building material of choice; promote international best practice in the areas of safety, production and the use of cement and concrete in the built environment; foster innovation in the cement and concrete sectors; make a positive contribution to global sustainable development; and promote the principles of a circular economy across the value chain.
"Concrete is the enabler of critical buildings and infrastructure that enhance the way we live – safe and durable homes, roads, hospitals, clean water, effective wastewater management, as well as providing the vital structures for the clean energy of tomorrow," said Benjamin Sporton, the CEO of the GCCA.
The association was launched in January 2018. It represents 32 member companies with nine affiliate organisations. Its members hold 35% of global cement production.
Philippines: Cemex Philippines' subsidiary APO Cement plans to close its Davao cement terminal and indefinitely suspend one of its kilns at its Barangay plant in Cebu. It said in a statement that it had taken this action due to uncertainty caused by the disruption to its raw material supply, according to GMA News. It follows the on-going suspension of APO Land and Quarry following a landslide in September 2018. APO Land & Quarry supplies raw materials to APO Cement.
Philippines: Apo Cement is preparing to temporarily lay-off up to 30% of its employees and 40% of its contractors. It has filed a formal notice detailing its intentions with the Department of Labor and Employment in Central Visayas, according to the Philippines News Agency. It says it has been forced into reducing its workforce in response to the on-going suspension of Apo Land and Quarry following landslides in September 2018. APO Land & Quarry supplies raw materials to CHP's subsidiary Apo Cement, and it is indirectly 40% owned by Mexico's Cemex.
HeidelbergCement is set to release its third quarter financial results later this week. In the meantime what can the results from the other major cement producers tell us?
Graph 1: Revenue from major cement producers, Q1 -3 2018. Source: Company reports.
The biggest of the big beasts, China National Building Material (CNBM), released its third quarter update last week. As usual for a major Chinese producer it was the expected story of continuing double-digit growth. Operating income up, profit up and little other information besides.
CNBM's half-year report back in August 2018 had more information, revealing that cement production volume fell by 5% year-on-year to 143Mt in the first half of 2018 from 150Mt in the same period in 2017. This was pinned on 'flat' demand, increased pressure on environmental protection and rising costs of fuel and raw materials. As we mentioned at the time the state-owned company is attempting to cope with the aftermath of China's great construction boom. National Bureau of Statistics (NBS) data shows that local cement sales dropped by 8% year-on-year to 158Mt in the first nine months of 2018. CNBM's cement sales are likely to have dropped also so far in 2018 but continuing industry consolidation and/or the merger with Sinoma may save them. With this in mind note the lack of sales volumes figures from CNBM and Anhui Conch in Graph 2 below.
Graph 2: Cement sales volumes by major cement producers, Q1 -3 2018. Source: Company reports.
Of the other larger Chinese producers, Anhui Conch's third quarter report was similarly sparse, sticking to the facts (revenue and profit up) and discussing in more detail a recent large-scale sale and purchase agreement with Jiangsu Conch Building Materials with a value of up to around US$230m. China Resources Cement is typically more verbose in its results releases. Its turnover and profits are also up so far in 2018 but it actually explained that cement and clinker prices had risen by 32%.
As for the others, both Cemex and UltraTech Cement are looking good so far. Growth in Mexico and the US has bolstered Cemex's performance giving, it a 7% year-on-year boost to US$10.9bn in the first nine months of 2018. Cement sales volumes grew more slowly at 3%, although operating EBITDA remained flat. Part of this was down to poorer markets south of Mexico, notably in Colombia. UltraTech Cement is still looking good after its acquisition of Jaiprakash Associates' plants in 2017 but earnings and profits have started to decline. The Indian market leader has blamed this on mounting energy and logistics costs coupled with local currency depreciation effects.
So, in summary, generally good news from the big producers, although issues are present in certain markets, notably South America. HeidelbergCement has already set the scene for its third quarter results with a warning that its earnings are down due to poor weather in the US and rising energy costs. Sales volumes and revenue are said to be 'within expectations.' Its Indian subsidiary, HeidelbergCement India, reported storming figures for its half-year to the end of September 2018 with double-digit growth across sales, sales volumes and earnings. Less reassuringly, its larger Indonesian subsidiary reported falling sales for the first nine months of 2018. All eyes will be on HeidelbergCement later in the week to see how this plays out.
Mexico: Cemex says that its digital platform, Cemex Go, has reached over 20,000 customers in 18 countries in the first year of its operation. This figure represents about 60% of Cemex's total recurring customers worldwide or about 20% of its global sales. The system allows the company and its customers to manage order placement, live tracking of shipments and invoices and payments for the company's main products, including bagged and bulk cement. Cemex also expects that analytics data from the platform will enable it to make efficiency savings.
Neoris is also helping to commercialise the platform to other heavy building material companies in partnership with IBM. This builds upon Neoris and IBM's experience helping Cemex develop and launch the digital product.
Spain: The Ministry of Industry and two unions have asked Cemex to keep the Gádor cement plant in Almería open. However, the Mexican cement company has rejected the pleas although it has said it will make a 'definitive' decision shortly, according to the Expansión newspaper. The company is due to start mandatory consultations with the unions in early November 2018. Cemex announced in mid-October 2018 that it was closing two of its seven cement plants in the country.
Mexico: Sales growth in the US and Mexico has contributed to a strong third quarter for Cemex in 2018. Overall, its net sales rose by 7% year-on-year to US$10.9bn in the first nine months of 2017 from US$10.2bn in the same period in 2017. Cement sales volumes rose by 3% to 52.7Mt from 51.1Mt. However, despite the sales growth, operating earnings before interest, taxation, depreciation and amortisation (EBITDA) remained flat at US$1.96bn.
"These results were underpinned by healthy volume and pricing dynamics in our three core products in most of our portfolio. We are pleased with our operations in Mexico and the US, with strong growth in year-over-year volumes for our three core products and improved prices. In our Europe region, prices continued to improve with growth in ready-mix and aggregates volumes. In addition, in our Asia, Middle East and Africa region, we saw volumes and prices in the Philippines rising in the mid-single digits as well as a double-digit increase in cement prices in Egypt," said Fernando A Gonzalez, chief executive officer (CEO) of Cemex.
Despite the strong markets in North America the building materials company reported a 3% drop in net sales in its South, Central America and Caribbean business area. A particular poor result was noted in Colombia. However, cement sales volumes picked up year-on-year in the third quarter of 2018 following elections.
Well, it turns out that the European cement industry wasn't kidding when it raised the risks of the climate mitigation on the sector. This week three (!) integrated plants have been earmarked for closure.
Cementa in Sweden said that it was considering closing its Degerhamn plant due to increased environmental regulations. Today, local press in Spain is reporting that Cemex España is planning to shut down two of its plants. These are plants in different parts of Europe with different local market dynamics but both are within the European Union (EU). That's three plants closing out of 219 in the EU, or a loss of around 1% of production capacity.
These words are similar to the comments Albert Scheuer, a board member of HeidelbergCement, made at the Innovation in Industrial Carbon Capture Conference early in 2018 about dividing the mounting environmental costs of cement and concrete between producers and society in general. Considering how much cementitious building materials most people use throughout their lives compared to the relative low price of cement, this argument carries some weight. In addition, the sustainability credentials of concrete buildings through longer lifespan and durability through extreme weather events is another argument that industry advocates such as the Portland Cement Association (PCA) in the US have been hawking in recent years.
Cementa, a subsidiary of HeidelbergCement, blamed anticipated tightening of environmental regulations for its decision. Although it said that the plant had made improvements over the years, the expected difficulty (read: cost) to make further improvements was becoming too hard. Shifting production to the company's other two plants in the region, Slite on Gotland and Brevik in Norway, will reduce CO2 emissions by 260,000t/yr.
In Spain, the news from Cemex follows a half-year report from Oficemen, the local cement association, that predicted growth for the year but not as fast as previously expected. The problem was that continued declines in the export market, the 13th decline month-by-month in a row, offset the domestic growth. Oficement president Jesús Ortiz also took time to blame rising electricity costs, expected to rise by 20% year-on-year by the end of 2018.
Market issues in Spain aren't in doubt, but the real question for both Sweden and Spain is whether EU CO2 legislation right now is causing cement producers to shut plants. The CO2 emissions allowance price hit a high of Euro22/t in September 2018, the highest price in a decade. Allowances have stayed below Euro10/t since 2011 and the price has more than doubled in 2018. Throw in the mood music of the IPCC and the trend seems irresistible. How many more plants in Europe are at risk to shut next? No doubt the European cement producers have charts marking the viability of their plants against the CO2 price. This would be a very interesting graph to get our hands on.
Spain: Cemex España is preparing to close its cement plants at Gádor in Almería and Lloseta in Baleares. It has blamed reduced demand for cement and European regulations on CO2 emissions for the decision, according to the Cinco Días newspaper. The closures will affect 200 employees and the cement producer is has started to hold union discussions. Cemex will retain integrated plants at Morata de Jalón, Alicante, Alcanar, Castillejo Anover and Buñol.


text:
See & Do Natural landscapes and sights
New Year's rejuvenation
Forget sitting around trying to recover from Christmas, Ireland has the perfect ways to rejuvenate your soul for the New Year
It's January. We've all eaten too much. So this month is supposed to be all about a diet of alfalfa sprouts, Spartan living and a few quick-fix detoxes, right?
Well, not in Ireland. As the New Year kicks in, the only way to face January is with a brave face, a rejuvenated soul and an active mind. And we have the perfect ways to achieve New Year bliss.
1. Soaking your way back to better health
Who said the New Year had to mean monastic-style self-denial? In Ireland you can avail of indulgent therapies that are satisfyingly virtuous at the same time. Enter the seaweed bath. Popular at seaside resorts all over the island in Edwardian times, hopping into a warm tub of freshly harvested seaweed is fashionable once more.
Why? Well, it all has to do with the therapeutic benefits of Irish seaweed, which has excellent detoxifying properties and makes your skin feel super-soft and supple. At VOYA Seaweed Baths in scenic Strandhill, County Sligo you can experience all manner of deluxe treatments: from a simple seaweed baths and steam, to an Organic Seaweed Leaf Wrap.
The Connemara Seaweed Baths in the wilds of Killary Harbour in County Galway keeps it old-school with salt-water seaweed baths in treatment rooms that overlook a beautiful fjord. Or enjoy a dose of Victorian elegance at the award-winning SOAK Seaweed Baths in the coastal village of Newcastle, County Down, with accommodation and seaweed baths sessions.
VOYA Seaweed Baths, County Sligo
2. Soulful stretching in a scenic wilderness
Grabbing your yoga mat and heading to an urban yoga class is good, but we can do better. If your body and soul is in need of soothing, then there is nothing quite like a yoga retreat in the middle of exceptional, and we mean exceptional, scenery.
Picture it: great yoga classes, views of the wilderness, a soothed soul… Located in the stunning Burren region of western Ireland – a place with a unique ecosystem and undulating limestone plateaus that spill down into the Atlantic – is Burren Yoga. It's yoga-retreat heaven.
On a small island near the entrance to Clew Bay in County Mayo is an island that is defined by incredible cliffs, swirling sea birds, hills, bogs and forests. And in the middle of all this, you'll find Clare Island Retreat Centre, a fantastically remote escape in which to soothe your weary soul.
And if you want to add in an extra dose of spirituality, then the retreat centre of Mandala House should fit the bill. Overlooking the glassy tranquil waters and islands of Upper Lough Erne, County Fermanagh is a retreat centre that will boost your energy levels with power yoga and calm your addled mind with meditation.
3. Get energetic with a walking adventure
January is the time to get out there and get active; to get your blood pumping and to see sights that will restore your faith in the world. And that means walking. But not just any walking; we're talking walks through some of the most inspirational scenery in western Europe.
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Ireland's coasts serve up something special, and gusts of salty sea air mixed with epic scenery is just the thing to get you back after Christmas. There are incredible walking routes all over the island, such as the wild and enigmatic routes of the Beara Way and the Sheep's Head Way in West Cork, where trails will bring you to the edge of sea cliffs, through boggy fields and to the very tip of peninsulas that jut out into the Atlantic Ocean.
And there couldn't be a better, or quieter, time to walk the world-famous Causeway Coast Way that runs from Portstewart to Ballycastle, with sweeping views of broad bays, sandy beaches and seriously dramatic cliffs.
4. Fire up your spirit by learning something new
Ireland not only offers to you the chance to learn, or try, something new. But it guarantees exceptional scenery in which to do it. Add to that a friendliness that has become world famous, and learning a new skill in Ireland is something to savour. There's no better place to unleash your creative passions – this is an island that holds literature, art and music close to its heart. According to Irene Graham of the Creative Writers Workshop in Connemara, "Raw beauty, comfortable surroundings and good food combined with creative writing workshops allow the writer to draw upon their unconscious, create and write."
Why not try a pottery workshop at Arran Street East in Dublin; cookery classes at the super-hip James Street South restaurant and cookery school in Belfast; or get your friends together for some traditional Irish music classes with The Bodhrán Experience.
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As the focus on fundamental science and knowledge over the past decade has now begun to produce dividends demonstrated by the number of nanotechnology-enabled products and market growth, nanomanufacturing remains the essential bridge between the discoveries of the nanosciences and the commercialization of nanotechnologies. Nanomanufacturing, defined as the controllable manipulation of materials structures, components, devices, and systems at the nanoscale (0.1 to 100 nanometers) in one, two, and three dimensions for large-scale reproducibility of value-added components and products, seeks to accelerate the proliferation of nanotechnology enabled products through the development of new process methodologies, tools, materials, and systems that are becoming established within the global manufacturing base. In this manner, many new products, markets, and processes will benefit from value-added commercial products enabled by the collective performance of their nanoscale building blocks. As the focus on fundamental science and knowledge over the past decade has now begun to produce dividends demonstrated by the number of nanotechnology-enabled products and market growth, nanomanufacturing remains the essential bridge between the discoveries of the nanosciences and the commercialization of nanotechnologies. Nanomanufacturing, defined as the controllable manipulation of materials structures, components, devices, and systems at the nanoscale (0.1 to 100 nanometers) in one, two, and three dimensions for large-scale reproducibility of value-added components and products, seeks to accelerate the proliferation of nanotechnology enabled products through the development of new process methodologies, tools, materials, and systems that are becoming established within the global manufacturing base. In this manner, many new products, markets, and processes will benefit from value-added commercial products enabled by the collective performance of their nanoscale building blocks.


text:
\section{Introduction}

Most luminous infrared (IR) galaxies (LIRGs; 10$^{11}$ L$\rm
_\odot$ $<$ L$\rm _{IR}$ $\leq$ 10$^{12}$ L$\rm _\odot$) are found
in interacting or merging systems with disturbed morphologies. In
the standard scenario proposed by Sanders et al. (1988a,b), the
formation of LIRGs, or ultra-luminous infrared galaxies (ULIRGs)
is due to the interaction and merging of two gas-rich galaxies.
Numerical simulations of interacting galaxies
\citep{barnes91,mihos96} indicate that a stable bar is formed
during the first encounter. Under the gravitational torque induced
by the bar, the molecular gas is channelled into the central
regions of the galaxies forming a huge reservoir to fuel intense
starbursts. Recent high angular resolution observations \citep{downes98} seem to support
this picture by revealing rotating disks of molecular gas that has
been driven into the centers of the mergers.

A lot of (U)LIRGs have been studied at high angular resolution, for example
ARP~299 \citep{casoli99}, NGC5394/95 \citep{kaufman02}, ARP~220 \citep{wiedner02},
NGC4038/39 \citep{zhu03}, NGC5194/95 \citep{matsushita04}, NGC~6090 \citep{wang04},
NGC5218 \citep{olsson07}. A few samples of the sources along the merging sequence
are also been investigated. \citet{xilouris04} found evidence for an increase
in 100- to 850-$\mu$m flux density ratio along the merging sequence and
interpreted this trend as an increase of the mass fraction of the warm dust in
comparison to the cold dust, inferring the possible enhanced star formation
rate (SFR). \citet{bergvall03}, however, question the
ubiquitous connection between interactions and starburst activity.
\citet{gao99} find the enhanced star formation efficiency (SFE) for
the later merging systems, but the effect is cancelled by the decrease
in the amount of molecular gas. That might result in no change in the infrared luminosity, i.e.
the indicator of the starburst activity. Thus more sources in high
resolution are needed and multiple CO transtions are essential to
investigate the gas properties for the mergers at different
stages.

Here we present another case study of an early merger system,
ARP~302. This galaxy is also named as VV 340 or UGC 9618, which consists of two galaxies
(ARP~302N and ARP~302S) with a separation of about 40$\arcsec$ between the two
nuclei, which is $\sim$27 kpc at the angular distance of 138 Mpc
(the luminosity distance is 147 Mpc), and has an infrared
luminosity of 4.5$\times$10$^{11}$ L$_\odot$. ARP~302 is the most
CO luminous system known in the local universe, and more luminous
in CO than those ultraluminous galaxies out to redshifts of 0.27
(Solomon et al. 1997). The detected molecular gas mass is
9.1$\times$10$^{10}$ M$_\odot$ \citep{lo97} (corrected by the adopted
comsmology here). HI data gives a mass
of atomic hydrogen 2.7$\times$10$^{10}$ M$_\odot$ \citep{van01}.
In all observations it was found that
ARP~302N contributes most of the IR emission and molecular gas
mass.

Previous high resolution CO $J$=1$-$0 observation on ARP~302 by
\cite{lo97} (the angular resolution is
7$\arcsec$$\times$5$\arcsec$) reveals two extended CO disks ($>$
10 kpc), and ARP~302N shows roughly an exponential disk with a
scale length of 7 kpc extending out to 23 kpc in diameter.
Based on the unusually extended distribution of the molecular gas,
\cite{lo97} concluded that the high IR luminosity in ARP~302
arises simply because an extremely large amount of molecular gas
is forming high-mass stars at a rate similar to the Galaxy, instead of the
starburst activities in the galactic nucleus.

In this study, we report the high angular
resolution CO $J$=2$-$1 observation of ARP~302N and the analysis of archival
data in the radio and mid/far infrared to study the physical properties of the gas
as well as the star formation activities in this early merger. In \S\ref{observations},
we show the details of our observations together with the
information about the archive data used in this paper. In
\S\ref{spatial}, \S\ref{ratio} and \S\ref{kinematics}, we present
the results of spatial distribution and the kinematics of the
molecular gas of our observations. In \S\ref{vla} and
\S\ref{spitzer}, the results of the radio emission and the mid/far
infrared emission from the archive data are presented. Finally we
present the dust properties using a dust model in \S\ref{dust},
the excitation condition of the gas in \S\ref{excitation}, the
star formation activities in \S\ref{formation} and a comparison with
other mergers in \S\ref{compar}. A summary of this
study is given in \S\ref{conclusion}. In this paper, we use a
$\Lambda$ cosmology with $\rm H_{\rm0} =
71$~km~s$^{-1}$~Mpc$^{-1}$, $\rm \Omega_\Lambda=0.73$ and $\rm
\Omega_{m}=0.27$ \citep{spergel03}.

\section{Observations}\label{observations}

\subsection{CO $J$=2$-$1 observation with the Submillimeter array}

We carried out the observation of the CO $J$=2$-$1 line from
ARP~302N on 2005 March 26, using the Submillimeter array
(SMA\footnotemark[5])\footnotetext[5]{The Submillimeter Array is a
joint project between the Smithsonian Astrophysical Observatory
and the Academia Sinica Institute of Astronomy and Astrophysics,
and is funded by the Smithsonian Institution and the Academia
Sinica.} \citep{ho04} in its most compact configuration. At that
time the SMA consists of 7 antennas of 6 meter in diameter. The
weather condition during our observations is average, with
atmospheric opacity at zenith $\tau_{225}$ $\sim$ 0.35. The single
sideband system temperature is about 450 K. Because of the large
extent of ARP~302N, we cover the whole galaxy using a two-pointing
mosaic, with a separation of 20$\arcsec$ between the two pointings
located at 10$\arcsec$ north and south of the nucleus
($\alpha$=14$^h$57$^m$00$^s$.67, $\delta$=+24$\rm
^o$37$\arcmin$02$\arcsec$.8).

The total on-source time was about 2 hours per one pointing. We
observed the CO $J$=2$-$1 line in the upper sideband of the double
sideband receiver. The SMA digital correlator was configured to
provide twenty-four independent spectral windows in each sideband.
Each window was divided into 128 channels, which provided 0.8 MHz
frequency resolution (i.e. $\sim$1.1~km~s$^{-1}$) at 223 GHz,
giving a total frequency coverage in each sideband of 1.97 GHz
(i.e. $\sim$2650~km~s$^{-1}$). We tuned the SMA receivers to the
redshifted CO $J$=2$-$1 line at the frequency of 222.967 GHz,
which corresponds to the systemic velocity of 10180
\ifmmode{{\rm \ts km\ts s}^{-1}}\else{\ts km\ts s$^{-1}$}\fi. We observed Jupiter and Callisto for bandpass and flux
calibration respectively, and estimated the flux density scale to
be accurate to about 10\% at 1.3 mm band. The nearby quasar
1357+193 was observed every 20 minutes to correct for
time-dependent gain variations due to atmospheric fluctuations.
The data were calibrated using the MIR-IDL package, which was
specially developed for the SMA. We then exported the data into
MIRIAD format for further processing. The mosaiced images made
from SMA data were deconvolved using the Steer-Dewdney-Ito clean
algorithm \citep{steer84}. The synthesized beam size is
3.4$\arcsec$$\times$2.5$\arcsec$ for the CO $J$=2$-$1 observatrion
with the uniformed weighting and the resulting noise level is 60
mJy beam$^{-1}$ at a velocity resolution of 20 km~s$^{-1}$. The 230
GHz continuum image of ARP~302N was formed from the line-free
channels and the rms noise level is 5 mJy~beam$^{-1}$.
No 1.3 mm continuum emission was detected from our
observation at 3 $\sigma$ level of 15 mJy~beam$^{-1}$.

\subsection{CO $J$=2$-$1 observation with the Submillimeter Telescope}
To estimate the amount of CO J=2--1 flux recovered in our SMA
observations, we also observed the CO $J$=2$-$1 line in ARP~302N
with a single dish telescope, the Submillimeter Telescope (SMT),
in Arizona on 2005 December 14 under excellent weather condition
($\rm \tau_{225 GHz}$ $\sim$ 0.08). The observation was done in
beam switching mode, with a beam throw of 2 arcmins and a chopping
frequency of 1.25 Hz. The half-power beamwidth (HPBW) of the SMT
telescope at the frequency of CO J=2--1 line is 28$\arcsec$, which
is large enough to cover most of the CO emitting region of
ARP~302N. The acousto-optical spectrometer (AOS) was used as the
backend, with a usable bandwidth of 1 GHz and a velocity
resolution of 1.3~km~s$^{-1}$. A single pointing observation was
made toward the nucleus of ARP~302N. The on-source integration
time was 45 minutes. The data was reduced with the GILDAS software
package. All the spectra were then co-added to produce the final
CO J=2--1 spectrum of ARP~302N. The final spectra were smoothed to
the resolution of 14 km~s$^{-1}$. The
noise level on antenna temperature scale was 3 mK. We
converted the spectrum into main beam temperature scale using a
main beam efficiency of 0.66.

\subsection{VLA archive data}
We searched the Very Large Array data archive, which is provided by the National Radio Astronomy
Observatory
(VLA\footnotemark[6]\footnotetext[6]{The National Radio Astronomy
Observatory is a facility of the National Science Foundation
operated under cooperative agreement by Associated Universities,
Inc.}), for data on ARP~302N. Previous observations were found for
X band (8.44 GHz, i.e. 3.6~cm), C band (4.86 GHz, i.e. 6.0~cm) and
L band (1.49 GHz, i.e. 20~cm). We used the NRAO data reduction
package to reduce the available data sets. Continuum images were
made using a natural weighting. For X-band data, which were obtained in
the extended configuration, we
applied tappering to the data in order to recover the more extended continuum emission.

\subsection{Spitzer archive data}
To compare with our SMA data, we also searched for the archival
data on ARP~302N produced by the Spitzer telescope. We found that
ARP~302N was imaged with the Infrared Array Camera (IRAC; Fazio et
al. 2004) in all four channels (3.6, 4.5, 5.8, and 8.0 $\mu$m) on
2005 July 16 and with Multiband Imaging Photometer for Spitzer
(MIPS; Rieke et al. 2004) in 24, 70 and 160 $\mu$m on 2005 January
25. The images were reduced with the Spitzer Science Center (SSC)
IRAC reduction pipeline and combined with the SSC mosaicker. The
point spread functions are
2.2$\arcsec$, 6$\arcsec$, 18$\arcsec$ and 40$\arcsec$ for 8, 24,
70 and 160 $\mu$m wavelengths, respectively. We only use the 8.0 $\mu$m and
the MIPS data in this paper. The uncertainties on the final
absolute calibrations are estimated at 10\%, 10\%, 20\%, and 20\%
for the 8, 24, 70, and 160 $\mu$m data, respectively.

\section{Results}\label{results}

\subsection{Spatial distribution of the molecular gas}\label{spatial}

In Figure~\ref{channel_map} we show the channel maps of CO
$J$=2$-$1 emission for ARP~302N. There is a clear positional shift
of the emission centroid with the velocity along the north-south
direction, consistent with the rotation of the gas in the galactic
disk. In each velocity channel we find that the emission is just
barely resolved in the east-west direction, which is perpendicular
to the galactic plane. In the channels with the velocity within
$\pm$ 80 \ifmmode{{\rm \ts km\ts s}^{-1}}\else{\ts km\ts s$^{-1}$}\fi, the emission is compact and only slightly resolved
by the SMA, showing a symmetric distribution. The emission in this
velocity range is centered at the nucleus and the emission of some
channels is weaker than the channels outside this range. In higher
redshifted and blueshifted velocity channels the emission is
slightly more extended in the north-south direction, especially
for the channels above $\pm$ 220 \ifmmode{{\rm \ts km\ts s}^{-1}}\else{\ts km\ts s$^{-1}$}\fi. For the receding part of the
galaxy the CO J=2--1 emission is resolved into two distinct
components, which are separated by about 8$\arcsec$.

Because the total extent of the CO emission is significant by
comparison with the primary beam of the SMA, part of the CO flux
could be resolved out in our SMA observations. In
Figure~\ref{spectra} we compare the spectrum of CO J=2--1 obtained
with the SMT at the resolution of 28$\arcsec$ and that obtained by
convolving our SMA channel maps to the same resolution. The CO
$J$=2$-$1 flux detected by the SMA within one SMT beam centered at
the nucleus is 356($\pm$8) Jy km~s$^{-1}$. It suggests that the SMA
recovers about 60\% of the CO $J$=2$-$1 flux from Arp 302 in
comparison with a total flux of 576 Jy \ifmmode{{\rm \ts km\ts s}^{-1}}\else{\ts km\ts s$^{-1}$}\fi detected by the SMT. The
total CO $J$=2$-$1 flux detected by the SMA is 382 ($\pm$10) Jy
km~s$^{-1}$. The most significant difference between both spectrum
is the comparatively lower emission in the SMA spectrum from 220 to
320 \ifmmode{{\rm \ts km\ts s}^{-1}}\else{\ts km\ts s$^{-1}$}\fi, which could be due to extended emission that is partially
resolved out by the SMA in the outer northern region. The similarity
in the line shape between single dish and the SMA spectrum suggests
that the missing flux is more or less uniformly distributed across
the line.

Figure~\ref{arp302_color}(b) shows the contours of integrated CO
$J$=2$-$1 intensity map at 3.4$\arcsec$$\times$2.5$\arcsec$
resolution by the SMA. The molecular gas almost covers the entire
optical disk of the galaxy seen almost edge on and distributes
over a region with the size of about 15 kpc. We find that the
molecular gas has a very asymmetric distribution with two strong
concentrations on either side of center together with a outmost
weaker concentration offset by about 8 kpc to the north. In the
figure, we show three crosses from bottom to top: one is at the
nucleus, the second is at the peak of 3.6 cm emission outside of
the nucleus (see \S\ref{vla}) and the third one is at the outmost
north for the weak CO J=2--1 emission concentration. To compare
with the BIMA data, we show the BIMA CO $J$=1$-$0 map in
Figure~\ref{arp302_color}(a). Our higher resolution map allows us
to investigate the molecular gas distribution with three
concentrations along the north-south direction, which the BIMA
data can not tell us. We also convolved the SMA beam to the BIMA's
and the map is shown in Figure~\ref{arp302_color}(d).
The BIMA map shows more extended distribution of the gas with large
radial distance comparison with the SMA result, which may be
due to the different exciation conditions for the gas at large
radial distance.

\subsection{CO $J$=2$-$1/$J$=1$-$0 line ratio}\label{ratio}

In Figure~\ref{arp302_color}(e), we present the map of the brightness temperature ratio of CO
$J$=2$-$1 emission from the SMA to CO $J$=1$-$0 emission from the
BIMA. To calculate the line ration, we first convolve our CO $J$=2$-$1 map to the same
angular resolution of 7$\arcsec$$\times$5$\arcsec$ of the BIMA
data as shown in Figure~\ref{arp302_color}(d) and form the line ratio map. We find that the line ratio varies from
0.2 at the outer region to about 0.5 at the peaks. The ratio
should be the lower limit since the missing flux of the SMA is
about 36\% but there is no missing flux for the BIMA data -- the
flux of 304$\pm$45 Jy km~s$^{-1}$ from the BIMA CO $J$=1$-$0
observation \citep{lo97} is similar to the value of 290$\pm$35 Jy
km~s$^{-1}$ from NRAO 12m telescope (private communication from Y.
Gao; Gao \& Solomon 1999). The line ratio is a very important observational
constraint to estimate the physical conditions of the molecular gas in
Arp~302N as we will show in the next section.

\subsection{Kinematics}\label{kinematics}

We present in Figure~\ref{arp302_color}(c) the intensity-weighted velocity
field as contours. A velocity field typical of normal rotation is clearly
seen along the major axis within a radius of $\sim$4$\arcsec$, i.e. 2.7~kpc.
Along the minor axis, we can not detect any disturblance of the gas in the inner
region. In Figure~\ref{velplot} we shows the position-velocity (PV)
diagram of the CO J=2--1 emission along the major axis (position
angle of 1$^\circ$). We note that the molecular gas exhibits a
nearly constant velocity gradient (about 100 km~s$^{-1}$
kpc$^{-1}$) within the central 6$\arcsec$ or 4.0 kpc in linear scale.
In the velocity range
between 260 and 340 km~s$^{-1}$ there are clearly two components: one is associated
with the gas at ARP302N-cm and the other component located to the
northern part about 8$\arcsec$ to 15$\arcsec$ away from
the nucleus. The gas at 3.3$\arcsec$ (2.2 kpc) north of the
nucleus shows a slightly steeper velocity gradient (about 170
km~s$^{-1}$ kpc$^{-1}$) and the position of this feature is
consistent with ARP302N-cm (the secondary 3.6 cm radio emission
feature, see \S\ref{vla}). The molecular gas located at large
galactocentric distance toward the north shows clear deviation from
solid body rotation, as can be seen in Figure~\ref{velplot}.

\cite{Sakamoto99} find that there is a steep rise in rotation
velocity, i.e. the velocity gradient $\sim$ 1000 km s$^{-1}$
kpc$^{-1}$, in the central regions with radii of typically
$\leq$ 0.5 kpc towards most nearby spiral galaxies.
It is therefore apparent that the presence of a shallow velocity
gradient over an extended region of 4.0 kpc in radius sets Arp~302N apart from
normal cases. However, solid body
rotation over kpc-scales is found in some special cases, such as NGC~4194 \citep{aalto00},
NGC~7479 \citep{laine99}, UGC~2866 \citep{huettem99} and NGC~891 \citep{garcia95}.
Usually the presence of a molecular ring
or the solid body rotation in bars are evoked to explain the observed linear velocity gradient.
\subsection{VLA results}\label{vla}
Low resolution of the images at C band (6~cm) and L band (20~cm),
as shown in Figure~\ref{arp302_vla}, indicate that
the radio emission is concentrated in the central region. There is
only one central peak and the details can not be well resolved
with the current poor resolutions, which are 13--14$\arcsec$ for
both observations. The integrated intensities are 30.2$\pm$0.4 mJy
and 89.0$\pm$3.6 mJy for 6~cm and 20~cm respectively, yielding a
spectral index, $\alpha$ (where S $\varpropto$ $\nu^{-\alpha}$),
of 0.9.

High resolution of the X band (3.6~cm) images are shown in
Figure~\ref{arp302_vla}. 3.6 cm continuum emission is mainly
contributed from two components with similar total integrated
intensity. One component, associated with the galactic nucleus, is
compact and marginally resolved (right top panel of
Figure~\ref{arp302_vla}). A second component is located at
3.3$\arcsec$ ($\sim$ 2.2 kpc) north of the nucleus (ARP302N-cm
hereafter) and extends from 2$\arcsec$ to 4$\arcsec$ away from the
nucleus (left top panel of Figure~\ref{arp302_vla}). All the results
are summarized in Table~\ref{xband}.

\subsection{Spitzer results}\label{spitzer}

In Figure~\ref{irac} we show the mid infrared continuum emision from
Arp~302 at 8.0 $\mu$m and 24 $\mu$m taken with IRAC and MIPS instruments
of Spitzer. Both 8.0 $\mu$m and 24 $\mu$m images exhibit similar
morphology to that seen in the CO J=2--1 emission.
Hot dust traced by the 8.0 $\mu$m and 24 $\mu$m share the
similar spatial distribution as the molecular gas traced by the CO
J=2--1 emission. With a resolution of $\sim$7$\arcsec$ at 24
$\mu$m, ARP~302 is very well resolved. From the MIPS image we estimate the flux densities
of 0.32$\pm0.03$ Jy and 0.08$\pm0.01$ Jy for ARP~302N and ARP~302S
respectively. The flux densities are 5.16$\pm1.03$ Jy at 70 $\mu$m
and 5.08$\pm1.02$ Jy at 160 $\mu$m for ARP~302N respectively.
Applying the same flux ratio based on 24~$\mu$m between ARP~302N
and ARP~302S to the total IRAS flux densities of ARP~302, we
estimate 5.32$\pm1.60$ Jy at 60 $\mu$m and 11.6$\pm3.5$ Jy at 100
$\mu$m for ARP~302N.

\section{Discussion}\label{discussion}

\subsection{Dust properties constrained by one component dust
model}\label{dust}

The dust continuum allows us to investigate the properties of the
dust, such as the dust temperature and the dust mass. To model the
dust emission from ARP~302N, we use the IR continuum fluxes measured
by Spitzer MIPS at 70 $\mu$m (5.16$\pm1.03$ Jy) and 160 $\mu$m
(5.08$\pm1.02$ Jy), and also by IRAS at 60 $\mu$m (5.32$\pm1.60$ Jy)
and 100 $\mu$m (11.6$\pm3.5$ Jy) (see details in \S\ref{spitzer})
together with the flux density of 135$\pm24$ mJy at 850 $\mu$m
reported by \cite{dunne00}.

Assuming that the dust emission is optically thin, the flux
density of the dust emission is related to the dust temperature
and the dust mass by the relation: $\rm
S_{\nu}=(1+z)[B_{\nu}(T_{dust})-B_{\nu}(T_{bg})]\kappa_d(\nu)
M_{dust}/D_L^2$, where $\rm S_{\nu}$ is the observed flux density,
$\rm T_{dust}$ and $\rm T_{bg}$ are the dust and background
temperature respectively, $\rm B_{\nu}$ is the Planck function,
$\rm D_L$ is the luminosity distance of the source, $\rm M_{dust}$
is the dust mass and $\rm \kappa_d$ is the dust absorption
coefficient. For the dust absorption coefficient, we adopt $\rm
\kappa_d(\nu) = 0.4~(\nu/250~GHz)^\beta$ cm$^2$ g$^{-1}$, where
$\beta$ is the emissivity index. We note that the emisivity index
$\beta$ depends on the dust properties and needs to be specified
beforehand. By fitting the observational measurements, we can
derive the dust mass and dust temperature for each specified value
of $\beta$. In Figure~\ref{sed}, we show three fitting results
with ($\beta$, $T\rm _{dust}$, M$\rm _{dust}$) combinations:
$\beta$=1.0, $T\rm _{dust}$=36 K and M$\rm
_{dust}$=2.2$\times$10$^8$ M$_\odot$ (the best fit), $\beta$=1.5,
$T\rm _{dust}$=29 K and M$\rm _{dust}$=2.0$\times$10$^8$ M$_\odot$
(moderate $\beta$ value), and $\beta$=2.0, $T\rm _{dust}$=26 K and
M$\rm _{dust}$=1.1$\times$10$^8$ M$_\odot$ (the simple modified
blackbody fit). The dust temperature ranges from 26 to 36~K for
the different models. Previous two models gives a dust mass of
2.0-2.2$\times$10$^8$ M$_\odot$, which are twice of the value from
the simple modified blackbody model.

The simple modified blackbody model underestimates
the 850~$\mu$m flux density by $\sim$60\%, which indicates that either
additional cold component or modifications to the emissivity index
are needed or that the optically thin assumption is inappropriate.
Actually, the gas is very extended in this galaxy and should result in
the similar distribution for the dust emission. The dust emission is
still optically thin at 70~$\mu$m even if the dust is distribuated
over a region with a small radius of 1~kpc, with a dust mass of
2.0$\times$10$^8$ M$_\odot$,
thus the optically thin assumption should be correct in this galaxy.
In a large survey for local galaxies by \citet{dunne00}, the dust
emissivity indexes to the best fitting models are found to be
1.3$\pm$0.2 and they argued that the galaxies may contain a
significant amount of cold dust. For ARP~302N, an additional cold gas component
with a dust mass of 1.6--2.5$\times$10$^8$ M$_\odot$ and a dust temperature
of 20-15~K can conpensate for the lower predicted flux at 850~$\mu$m.
This results in a total
dust mass of 2.7--3.6$\times$10$^8$ M$_\odot$ dependent on the
temperature of the cold dust component.

The observed flux in CO $J$=1$-$0 \citep{lo97} is 304 Jy~\ifmmode{{\rm \ts km\ts s}^{-1}}\else{\ts km\ts s$^{-1}$}\fi for ARP~302N,
and the corresponding CO line luminosities are 1.6$\times$10$^{10}$ K~\ifmmode{{\rm \ts km\ts s}^{-1}}\else{\ts km\ts s$^{-1}$}\fi~pc$^2$.
This places ARP~302 to be the most CO luminous system known in the local
universe and possibly the most gas rich system. Usually, we can estimate
the gas mass using a standard conversion factor, 4.8~M$_\odot$ (K~\ifmmode{{\rm \ts km\ts s}^{-1}}\else{\ts km\ts s$^{-1}$}\fi~pc$^2$)$^{-1}$
in our Galaxy, and it leads to a gas mass of 7.7$\times$10$^{10}$M$_\odot$.
We derived a dust mass of 2.0-3.6$\times$10$^8$ M$_\odot$ from our dust models as above.
Adopting the gas-to-dust mass ratio of 150 in our Galaxy, this yields
the value of 3.0-5.4$\times$10$^{10}$M$_\odot$ for the gas mass.
Therefore, the gas mass estimates from the dust and the CO luminosity
are comparable within their uncertainties and lead to a gas mass of
5.4$\times$10$^{10}$M$_\odot$ (the mean value from two methods).

The theoretical prediction of the flux density of the continuum
emission at 1.3mm is less than 42 mJy from the above dust models.
The sensitivity of the continuum observation is 5 mJy beam$^{-1}$,
thus it is reasonable that there is no positive detection from the
SMA observation if the emission is distributed over a region of
over 3 beams.

\subsection{Excitation condition of the gas}\label{excitation}

The excitation condition of molecular gas in ARP~302N can be
studied using the CO $J$=2$-$1/$J$=1$-$0 line ratio. As seen in
Figure~\ref{arp302_color} the line ratio peaks at either side of
the center. The ratio varies significantly across the galaxy, from
about 0.2 in the outer region to about 0.5 at the peaks. Assuming
that the missing flux of the SMA observation is uniformly
distributed, the line ratio will be 0.2 higher and the ratio will
vary from 0.4 in the outer region to about 0.7 at the peaks. The
overall line ratio from the single dish measurements is about 0.5.
From a survey of the CO $J$=1$-$0 and $J$=2$-$1 lines in the inner
kpc regions of a large sample of nearby spiral galaxies,
\cite{braine92} measured an average line ratio of 0.89, but
7 out of 35 galaxies have CO $J$=2$-$1/$J$=1$-$0 line ratios
less than 0.6. Furthermore, the gas in the central regions tend to
have high excitation temperature, which will result in the higher
line ratio if the CO line emission is optically thick.
The disks of NGC1808 \citep{aalto94} and our Galaxy show values
of 0.7 and 0.6, which are comparable to the value in the central
region of ARP~302N.

To be more quantitative, we use our molecular excitation model
to constrain the physical conditions of the molecular gas.
The transfer of radiation is calculated within the framework of
the large velocity gradient approximation. We take into account
all rotational levels of the CO molecule up J=10.
We use the collisional cross sections between CO and H$_2$ molecules
from \citet{flower85}. The statistical equillibrium equations
are solved using the Newton-Raphson method. In our molecular excitation model
three parameters are required: the gas density, the kinetic temperature and
the fractional abundance of the CO molecule per unit velocity gradient.
At the expected low density of the molecular gas, the kinetic temperature
is expected to decoupled from the dust temperature.
In this case, the kinetic temperature might be as low as half
of the dust temperature \citep{downes98}. In the previous section,
we estimate the dust temperature in the range of 26 to 36 K. For the
excitation calculation, we adopt two representative values of 20 and 30 K.
In Figure~\ref{lvg} (left panel) we present the dependence of CO
$J$=2$-$1/$J$=1$-$0 line ratio on the gas density $n({\rm H}_2)$
and the abundance per velocity gradient [CO]/$\rm{(dv/dr)}$ for
kinetic temperature of 20 and 30~K. The figure shows that for the line ratio
measured in ARP~302N the gas density is low, less than 10$^3$
cm$^{-3}$. At this low density, the transition $J$=2$-$1 is
sub-thermally excited. Lower line ratios correspond to lower
densities for a reasonable range of abundance per velocity
gradient. To provide further support for this conclusion we also
show the dependence of line ratio on the gas density and kinetic
temperature T$_{\rm kin}$ for a fixed abundance per velocity
gradient of [CO]/$\rm{(dv/dr)}$ = 1$\times$ 10$^{\rm -5}$ pc~($\rm
km s^{-1}$)$^{-1}$ (right panel of Figure~\ref{lvg}). The result
suggests only a weak dependence on kinetic temperature. Our
finding is very similar to the conclusion of \cite{sakamoto94} in
that the variation in line ratio mainly reflects the variation in
gas density. To set more stringent limits on the gas density and
temperature would require observations of higher transitions of CO
and/or its $^{13}$CO isotope.

The relatively low gas density in ARP~302N is reflected
in its spatial distribution. For ULIRGs, which are in a more
advanced merger phase, \cite{downes98} show that the molecular gas
is more strongly concentrated in the nuclear region of the galaxy in
the form of a rotating disk with size of 1 kpc or less. The
estimated average gas density is higher, ranging from a few 10$^3$
to 10$^4$ cm$^{-3}$. In ARP~302N, there is a large amount of
molecular gas (5.4$\times$10$^{10}$ M$_{\odot}$, see in \S\ref{dust}), but this gas is
distributed over a very extended galactic disk with a size of 15
kpc, resulting in lower average density.
We note that the diffuse and very extended spatial distribution
of molecular gas in ARP~302N is unusual among local luminous and ultralumious
galaxies. However, in some cases such as in the interacting galaxy M51, the molecular
gas traced by CO emission also covers all the optical disk,
out to at least 12 kpc radius \citep{schuster07}.
The origin of this distribution is currently unknown.

\subsection{Star forming activity}\label{formation}
The star formation activity can be estimated by SFE, the ratio of luminosity to molecular gas mass,
of the galaxies. For ARP~302N, we estimate an infrared luminosity
of 3.4$\times$10$^{11}$ L$_{\odot}$, separating the contamination
of ARP~302S in the manner described in \S\ref{spitzer}. We can
also estimate the infrared luminosity from the 24 $\mu$m data with
the empirical formula L$_{IR}$=10$\nu L_\nu(24 \mu m)$
\citep{bell05}, yielding a luminosity of 2.7 $\times$10$^{11}$
L$_{\odot}$, which is comparable with our estimated IRAS
luminosity. The molecular gas estimate is 5.4$\times$10$^{10}$ M$_{\odot}$
for ARP~302N. Its SFE of 6.3 L$_{\odot}$/M$_{\odot}$ is slightly
higher than that in our Galaxy but much
lower than starburst galaxies or (U)LIRGs. The high infrared
luminosity, the large amount of the gas mass and the low SFE make
this galaxy peculiar.

The SFR for ARP~302N is about 40 $\rm
M_\odot~yr^{-1}$ assuming SFR = 1.17$\times$10$^{-10}$ ($\rm
L\rm_{FIR}/L_{\odot}$) $\rm M_\odot$ yr$^{-1}$
\citep{kennicutt98}, and thus ARP~302N can retain such a
luminosity over a period of at most 2.0$\times 10^9$ yrs. The
system will likely evolve into advanced merger in a timescale of
several tens million yrs \citep{mihos96}, and may at that time
become a ULIRG with a luminosity of 1.6$\times$10$^{12}$
$L_{\odot}$ even if it will lose half of its gas mass by then
(given a SFE of 42 L$_{\odot}$/M$_{\odot}$ for the merging systems
with the separation less than 5 kpc from Gao \& Solomon 1999).

\subsubsection{Constraint from the line ratio}
As discussed in previous section, our excitation analysis suggests
that the low line ratio in ARP~302N is due to the low volume density
of the molecular gas. The low gas density is entirely consistent
with the low SFE observed in ARP~302N, as star
formation is associated with dense gas rather than just total gas
mass \citep{gao04}.

\subsubsection{Radio continuum}
The thermal radio emission from HII regions is identifiable by its
flat spectral index with a typical value of 0.1. A spectral index
of 0.9 as measured for ARP~302N implied that non-thermal emission
dominates. Synchrotron emission with a spectral index of 0.9 is
likely to be dominated by supernova remnants with small diameters,
referred to the star forming activity in ARP~302N. From the high
resolution images at 3.6~cm, the continuum emission mainly comes
from the nucleus and ARP302N-cm. Therefore, the nucleus and
ARP302N-cm are the regions with strong star forming activity.

\subsubsection{Strong star forming activities at the nucleus and ARP302N-cm}

The extended infrared emission from Spitzer 8 and 24 $\mu$m data
excludes the existence of a strong AGN in ARP~302N and favors the
star formation origin for the large infrared luminosity in
ARP~302N. Therefore it fully supports that the star formation
dominates the IR emission in the galgaxy. The 3.6 cm observation
shows that there is strong and extended radio continuum emission
at ARP302N-cm. The Spitzer 8 and 24 $\mu$m images peak at the same
region, indicating that there is strong emission from the PAH and
hot dust. The high resolution CO $J$=2$-$1 image from the SMA
reveals much molecular gas exists at ARP302N-cm. All of these
results support that there is the asymmetrical star forming
activities in the system and ARP302N-cm is the strongest active
star forming region in the galaxy.

From 3.6~cm images with the different
resolutions at the nuclear region, it is clear that at least 36\%
of the emission is not associated with the unresolved structure in
the nuclear region and 64\% of the emission is originated from a
compact region (from the VLA 3.6~cm data, the deconvolved size is
0.23$\arcsec$$\times$0.09$\arcsec$, i.e. 143 pc $\times$ 56 pc).
As a whole, the star formation is not active in ARP~302N, but there
is strong star forming regions at the nucleus and ARP302N-cm.

From the previous optical spectroscopy observation
\citep{veilleux95}, the system was classified as LINER type galaxy.
\citet{alonso00} claim that LINER-like optical
spectra would be the consequence of the shock-heating by supernovae
of the surrounding gas after a burst of star formation, as observed
in NGC~5218 \citep{olsson07}. This scenario to explain the LINER
type spectrum is consistent with our radio observation which suggests
that there are many supernova explosions. Of course, we can not
exclude the possible existence of a weak AGN in the center.

\subsection{Comparison with other mergers}\label{compar}
In Arp 302N the distribution and kinematics of molecular gas show no
discernable disturbance. That suggests the Arp 302 system is in the
early merging stage. Recently, many authors studied the molecular
gas in high angular resolution to investigate
the effects of the merging procedure and the star formation therein.
The molecular gas is often concentrated on the overlap region or at least have
another peak except for the centers of the systems with the well seperated nuclei,
such as ARP~299 \citep{casoli99}, NGC~6090 \citep{wang04} and VV~114 \citep{iono2004}.
In these cases, the starburst acitivites is prominent and the SFE is much higher
than that in our Galaxies. NGC~6670 is another widely seperated merger
and is well studied by \citet{wang01}. They also found that the stars
and the molecular gas do not show any clear sign of the
merging process. However, the atomic gas is found to concentrate in the region in between
the two galaxies, a very clear signature of the merging process.
The atomic gas will be helpful to determine the merging process in ARP~302.
Indeed, simulations show that the high SFRs and the SFEs arise only in the late
stages of the merger and the star formation does not deplete much gas
before it reaches the central regions in the mergering systems \citet{mihos94,mihos96}.
It is consistent with the observed enhanced SFE in the
late mergers by \citet{gao99}, which suggests that the fact before
its final merging stage is the reason why the SFE in this LIRG is just comparable to the
value in our Galaxy. The huge infrared luminosity in ARP~302N is just due to
its large amount of the gas mass instead of the starburst activity.

\section{Conclusion}\label{conclusion}
In this paper we present the SMA observations of the CO $J$=2$-$1
transition towards the northern galaxy, ARP~302N, of the early
merging system, ARP~302, to study the physical properties of the gas.
To well understand the star formation activities,
the VLA data at 3.6~cm, 6.0~cm, 20~cm and the Spitzer (both IRAC
and MIPS data) archive data are also shown here. Our main results
are summarized as the following:

\begin{enumerate}

\item Our high angular resolution CO $J$=2$-$1 observation reveals
the extended spatial distribution of the molecular gas in
ARP~302N. We find that the molecular gas has a very asymmetric
distribution with two strong concentrations on either side of the
center together with a weaker one offset by about 8 kpc to the
north. This spatial distribution is very similar to the morphology seen
previously in the CO J=2--1 line.

\item The distribution of the molecular gas is also found to be
consistent with that for the PAH and the hot dust as traced by the 8 $\mu$m
and 24 $\mu$m continuum emission observed by Spitzer.

\item The line ratio CO J=2--1/1-0 shows that the line ratio
varies strongly from about 0.7 near the galaxy center to 0.4 in
the outer part of the galaxy. Excitation analysis suggests that
the gas density is low, less than 10$^3$ cm$^{-3}$, over the
entire galaxy.

\item By fitting the far infrared part of the SED of ARP~302N, we obtain a dust
temperature $T\rm _d$ in the range 26--36 K and a dust mass of
M$\rm _{dust}$=2.0--3.6$\times$10$^8$ M$\rm _\odot$.

\item We determine the spectral index of the radio continuum to be approximately 0.9. The
spatial distribution and spectral index of the radio continuum
emission suggests that most of the radio continuum emission is
synchrotron emission from the star forming regions at the nucleus
and ARP302N-cm. The good spatial correspondance between the 3.6 cm radio continuum
emission, the Spitzer 8 and 24 $\mu$m data and the high resolution
CO $J$=2$-$1 observation from the SMA shows that there is the
asymmetrical star forming activities in ARP~302N and ARP302N-cm is
the strongest active star forming region in the galaxy.

\end{enumerate}

\acknowledgments

We would like to acknowledge the anonymous referee for the valuable discussions and
comments. We also thank the SMA staff for maintaining the operation of the array.
The SMT is operated by the Arizona Radio Observatory (ARO), Steward
Observatory, University of Arizona. Y.-P. Ao thanks the ASIAA for
supporting his stay as a Visiting Scholar, when much of this work
was done. Y.-P. Ao also acknowledge the support of NSFC grant 10733030.

redpajama_set_name: RedPajamaArXiv


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I've been reading about Dong Bei dumplings from various bloggers since last year but every time we go to Binondo, we always ended up eating at President's Tea House. The reason is we can't find Dong Bei's location from our few attempts, good thing the foodie-in-me kept on insisting to search for one of Binondo's best kept secrets.
Dong Bei is located at 642 Yuchengco St., from Binondo Church, walk down Ongpin St. and turn left at Yuchengco St. Dong Bei is next to a dress shop and it's nearing the dead end of the street. Although the restaurant's facade seems uninviting and unappetizing for a Chinese restaurant for that matter, based on the raves I read, it must be worth it.


Spinz.io in now available on your android device, the most recent spinz.io app is available on 9Apps ate there are over 10,000 downloads of this weekly! The app's been lend somewhat of a visual makeover, as well. This is a hot app that had been released in the month of July of 2017. You can get it for free.
When you use spinz.io app for playing the game on your android device you get an awesome multiplayer action game. This game has drawn inspiration from a trendy Fidget Spinner toy. As an io game, it bears a great deal of resemblance to a different trendy IO game, namely Agario. In view of this fact, the game concept is likely to be known to a good number of players. Just as in the game of Agar IO, each and every player has the job of collecting multicolored dots, dotted throughout the playfield.
The difference when playing the game of an android device with the spinz.io app from gar.io is that here the player has to control the fidget spinner! He/she must move his/her spinner all over the map and attempt to amass as numerous dots as likely. The picking up of dots helps a player gain RPM and the one player with the greatest RPM ends up as the leader of this game. The person's name is shown at the summit of the game rating list. The speedier the rotation of the spinner of a player is the greater the number of dots that it attracts.
You require collecting food, getting faster and crashing stronger.
You require showing your opportunities and getting into the game leader board, staying there for as long a time as probable for showing that you're even more awesome compared to the other spinners.
Your require moving liberally about the map, scoring an increasing number of RPM.
Sudden combats on the game map/ purposeful attacks by different players for getting your RPM, lends the game some unforgettable feelings and dynamics.
What's New in This Version Of The App?
Those who use the spinz.io app for playing the game on their android device would be glad to know that work in under progress for adding numerous pristine cool features!