text:
Lot Availability
A growing modern suburb with all the history of one of the oldest towns this side of the Mississippi.
"Liberty has the best combination of economic opportunity, good schools, safe streets, things to do, and a real sense of community."
— CNN/Money Magazine
THE CITY OF LIBERTY
Liberty, Missouri is a thriving suburb of Kansas City, Missouri that has been growing and developing since it's founding in 1812. Liberty has a history that encompasses everything from the Civil War to Joseph Smith, as well as Jesse James and the first daylight bank robbery. It has served as the Clay County seat since shortly after it's inception and has played in an important role in Missouri history throughout it's entire lifespan. The city has a strong culture of hometown pride and values it's history and cares about maintaining it.
Liberty has developed a reputation as one of the most liveable towns in Missouri. It is home to one of the top school districts in the state, an excellent liberal arts college, a historic downtown district, and all the modern amenities a resident could ask for.
Education is a vital element of every great small town and Liberty has opportunities at every level to have quality learning experiences.
LIBERTY PUBLIC SCHOOLS
Liberty Public Schools is consistently recognized as a top-flight district in Missouri. LPS has 11 elementary schools, four middle schools, two high schools, an alternative secondary school, and an early childhood center. The district serves 11,800 students and due to the rapid growth of Liberty, is the second fastest growing school district in the state. LPS has cultivated an atmosphere that prioritizes higher learning and 90% of graduates seek higher education. In recent years, LPS has been honored for their technological excellence and has been recognized nationally for their widespread implementation of technology to support education. A student who attends Liberty gets every chance to have a positive, successful education with the best teachers.
"LPS was recognized as a high performing school district for all 12 years the State of Missouri presented the Distinction in Performance Award, making it one of only 6% of Missouri districts to be placed in this category. "
— Liberty Public Schools
William Jewell College is a small liberal arts college founded in the mid 1800's. Jewell was named Liberal Arts "College of the Year" by Time Magazine and is widely recognized as one of the best liberal arts colleges in the nation. It maintains an attendance of approximately 1,000 students, and yet has a full complement of NCAA Division II athletics and a nationally recognized Fine Arts program. William Jewell also boasts:
65 percent of classes contain fewer than 20 students
More than 40 majors
Graduate Program (M.S.Ed. in Differential Education)
WHAT DOES LIBERTY HAVE TO OFFER
Living in Liberty gives you all the benefits of small town suburb living with easy access to the city of Kansas City.
Just north of Homestead lies the Liberty Community Center. The community center features an indoor/outdoor pool, a wonderful workout facility, basketball courts, as well as a 700 seat performing arts center which hosts numerous events throughout the year.
HISTORIC LIBERTY SQUARE
Discover a timeless blend of fascinating American history along with upbeat contemporary shopping and dining. Find a delightful mix of old and new from stores located in the architecturally beautiful buildings on the square to the unique shops of the restored Corbin Mill area to the many businesses nestled on side streets and byways.
Liberty has four excellent golf courses within 15 minutes of Homestead.
Cardinal Hill Golf Course
Liberty Hill Country Club
Shoal Creek Golf Course
HODGE PARK GOLF CLUB
Grab your clubs and enjoy a high quality golf experience at any of these award winning courses.
Hungry? Liberty offers easy access to a number of excellent restaurants, with new restaurants being added on a consistent basis.
"Liberty has been recognized as one of the Top 100 Small Communities (under 50,000) in the United States, one of the 10 Best Places to Raise a Family and as one of Missouri's top 10 towns by Missouri Life Magazine."
— The City of Liberty
homesteadofliberty@gmail.com
Make your next home a Homestead


text:
Narendra Modi, the leader of Bharatiya Janata Party, was sworn in as Chief Minister of Gujarat for the fourth time in 2012 following victory in 2012 Gujarat Legislative Assembly election.

Cabinet ministers
Babubhai Bokhiria
Bhupendrasinh Chudasma
Anandiben Patel
Nitin Patel
Saurabh Patel
Ramanlal Vora

Ministers of State
Pradipsinh Jadeja
Jayanti Kavadia
Govind Patel
Parbat Patel
Rajni Patel
Purshottam Solanki
Vasuben Trivedi
Liladhar Vaghela
Nanu Vanani
Ganpat Vasava

References

Modi 04
Modi IV
Chief Ministership of Narendra Modi
2012 establishments in Gujarat
Cabinets established in 2012
2014 disestablishments in India
Cabinets disestablished in 2014

redpajama_set_name: RedPajamaWikipedia


text:
Home/DC/'Doom Patrol' Seasons 1 & 2 Soundtrack Scores Released
'Doom Patrol' Seasons 1 & 2 Soundtrack Scores Released
Emre Kaya Follow on Twitter Send an email September 11, 2020
The official soundtrack score for DC Universe's and HBO Max's Doom Patrol has officially been released!
You can now listen to the soundtracks of Doom Patrol's first two seasons on all major music streaming platforms!
The season 1 tracklist includes:
Main Titles (Doom Patrol) – Clint Mansell, Kevin Kiner & Sean Kiner (1:14)
Aftermath in Cloverton (4:08)
Robotman and His Daughter (4:23)
Longing for Their Daughters (5:53)
Mr. Nobody and Willoughby (8:41)
Vic and His Traumas (3:49)
Larry and His Spirit (5:45)
Rita and Her Troubles (4:58)
Jane and the Underground (6:10)
Niles' Tales (7:04)
The Bureau of Normalcy (7:53)
Silas Knows the Truth (4:49)
The First Doom Patrol (6:37)
Vermin Patrol (7:57)
End Credits (Doom Patrol) – Clint Mansell, Kevin Kiner & Sean Kiner (1:08)
You can view the season 2 tracklist titles below:
Miniature Patrol (5:52)
The Candlemaker (7:48)
Father and Son (5:59)
Dr. Tyme and the Loose Brain (5:32)
Backstories (6:21)
Red Jack and the Butterflies (3:52)
To Keep Dorothy Happy (4:44)
Catching Sex Ghosts (4:22)
Cliff's Heroics (3:13)
Adventures in Space (6:33)
Scants (4:39)
It's Time (4:52)
Trauma at the Well (6:32)
Imaginary Friends (5:58)
Meet Your Fate (6:20)
You can find the soundtrack for the first season on Amazon, Spotify and Apple Music. For the second season, these are the Amazon, Spotify and Apple Music soundtrack links.
Doom Patrol is is developed by Jeremy Carver and stars Diane Guerrero, April Bowlby, Matt Bomer, Joivan Wade, Brendan Fraser, Alan Tudyk and Timothy Dalton. Both seasons of the show are now available to stream on DC Universe and HBO Max.
'Titans' Season 3 Production Update
'Titans' Season 3 Set To Start Production On October 13

redpajama_set_name: RedPajamaCommonCrawl


We provide various Home Inspection services across the entire Tampa Bay area and most can be customized to suit your needs.
We suggest a 4 hour time slot for Home Inspection and Reports are generated and available within 24 hours.
The cost for service is based on square footage of the home in addition to inspecting amenities such as a detached buildings.
APEX Home Allies has competitive pricing and can package services reasonably. You do have the option of making a payment from our website's "Make Payment" menu which will take you directly to PayPal's Secure Website. If you do not have a PayPal account you can use a Credit or Debit Card. Simply enter the amount, then click continue and you will see the option for Credit or Debit Card. Our office can also email you an invoice and you can pay using the secure link.


Use the journey planner above to find all travel options from Hannover to Mainz. Plan your trip, combine and compare transportation providers such as for example: Railway agencies, Bus operators. The accumulated distance between Hannover [LAT: 52.37589, LNG: 9.73201] and Mainz [LAT: 49.99286, LNG: 8.24725] is around 341.3 km. The trip to Mainz is around 4 hours 58 minutes by car if you are travelling from Hannover. Another way to enjoy your trip is to travel like the way locals do. For very short trips, we recommends taking bikes, taxis, subways, buses, etc. Use Combitrip to find efficient ways to travel on your trip. Door to door trip is best when there aren't any unpleasant surprises such as hidden charges or longer time to the airport/station. Combitrip eliminates these unpleasant surprises by providing detailed information of your options.


text:
San Franciscocalifornia-election-resultsCalifornia ElectionsVideo
California Prop 36, Measure Reforming State's Three Strikes Law, Approved By Wide Majority Of Voters
California's Three Strikes Law Strikes Out
Aaron Sankin
Assistant San Francisco Editor, The Huffington Post
Nov 7, 2012, 03:13 PM EST | Updated Nov 7, 2012
In this photo taken Jan. 12, 2012 inmates are seen in a recreation yard at the Deuel Vocational Institution in Tracy, Calif. California's realignment of its criminal justice system took effect nine months ago to address court-ordered reductions in overcrowding with the plan to shift thousands of those convicted of "non-serious" crimes to county jails. A new law changing where some criminals serve their time is prompting anger from certain lawmakers who believe the state again is reneging on its promise to keep those convicted of violent and other serious crime in state prison rather than county jails.(AP Photo/Rich Pedroncelli)
A ballot measure reforming California's Three Strikes Law was approved by a significant majority of California voters Tuesday, passing by the wide margin of 68.6 percent to 31.4 percent.
Before Tuesday's vote, state law allowed the imposition of a life sentence on an individual's third felony conviction. The revised law would require that the third offense be of a serious or violent nature--not something as minor as writing a bad check or, in a much-cited example, stealing a pair of socks.
"Tonight's vote on Proposition 36 sends a powerful message to policymakers in California and across the country that taxpayers are ready for a new direction in criminal justice,'' Adam Gelb, director of the Pew Center on the States' Public Safety Performance Project, told the San Jose Mercury News. "States that have already made some changes to their sentencing laws may be inspired to take a second look, and states that haven't made significant changes yet may start."
In addition to altering the sentencing guidelines for future convicts, Prop 36 also creates a pathway for nearly 3,000 inmates currently serving life sentences under the Three Strikes Law to petition for a reduced term.
California imposed its Three Strikes law in 1994 and it is widely considered one of the toughest such laws in the country. In the years since the law's initial passing, the state's prion population has swelled to unprecedented proportions: we now spend a larger percentage of its budget on prisons than on higher education.
Estimates have Prop 36 saving the state up to $90 million per year. As such, the measure was supported by both the San Francisco Green Party and anti-tax activist Grover Norquist.
Mike Reynolds, the author of the original Three Strikes law whose daughter was murdered by two habitual offenders, expressed concern that changes in the law would lead to increased crime. "It's a big day for criminals and their attorneys," Reynolds told the San Francisco Chronicle.
California voters amended the state's Three Strikes Law once before in 2000, passing a ballot measure directing certain non-violent drug offenders to treatment programs instead of prison terms.
Check out how all the other California ballot measures fared:
California 2012 Ballot Measures Results


There are many different dogs and many different families. It is hard to decide what to do about owning a dog. Keep reading to learn about your pet and its health.
When training a dog, practice in the yard or your home. Don't train in a park. They are going to become distracted, and the easiest commands can be tough.
Which breed you need to buy depends on your lifestyle. For instance, if you love to run, get a dog that loves to run too, and leave the miniature breed for someone who is less active. If you much prefer to be at home, a small dog that enjoys a lot of inside time is an ideal choice. Keeping a mismatch out of play makes both of you happy.
Be sure to praise your dog freely and consistently whenever he exhibits a desired behavior. You want to let your dog know that the behavior is something that you want to see. It will show your dog that doing the right thing will earn him praise from you.
Do not buy the cheapest dog food. Less expensive dog foods include fillers and additives that are not beneficial to your dog's health. Find a trusted group that offers a list of healthy dog food. Food that is healthy will benefit your dog.
Regularly brushing your dog's fur won't just stop your pet from shedding on your furniture. Brushing every day can also help your dog to have a shiny and beautiful coat. The brushing motion will distribute the oil through the dog's fur.
When you get a new dog, set up an appointment for him at the vet. When you bring them home, schedule a vet appointment. The vet is going to check over your dog to see if everything is okay, as well as set it up to get vaccinations it may need. Ask your vet about neutering your dog. Shelters are filled with unwanted animals and not neutering your dog means you could be making this problem worse.
If you are interested in adopting a pure breed, consider visiting the dog pound. Lots of dog owners will leave their dog stranded whenever they don't want it anymore. Contact the pound in your area to see what kinds of breeds they have at the time. You may even save a poor dog's life.
If you only have one dog and they aren't happy or can't handle being alone a lot, consider getting them a companion. Dogs naturally live in packs, and they are happiest when they are allowed to do so. Giving them some canine companionship can have a very positive effect on their mood and behavior. Find another dog that has the same energy levels and temperament and you'll be sure to find something your dog will love!
Do you feel relieved about caring for your dog right now? You have the right information, and now you just need to implement it. Use these tips to take proper care of the family dog.


We have multiple methods available to report violations of our safer spaces policy, with varying degrees of anonymity available. Event staff will take action as appropriate based on the details of the violation.
Event staff in red bandanas are prepared to take your report and, maintaining your desired level of anonymity, pass any necessary information on to Jesse and Zach.
You may call or text: 734-926-8507 with your report. This phone number is a google voice number that will ring down to trained staff members who will be able to assist you further.
Event staff will take appropriate action they deem appropriate based on the specific details of an incident. Action may include speaking to an individual about their behavior, removing an individual from the event, or contacting local authorities.


All of the adult members of In The Way Music Ministry are Virtus Trained and Certified in Protecting God's Children.
In The Way grew out of the Charismatic Community of St. Barnabas Parish in Bellmore, New York where we provide music support to the weekly prayer meetings. Over time we have branched out to serve other communities and play in other venues.
While the core members of the band are a constant, various venues add more members and bigger sounds. More information about the members of the group is available on our Band Biographies page.
Information regarding our current schedule (see right column) and the venues where we play is available on our Venues and Schedule page or see below for special events. Our Band News page also provides information about upcoming events and reviews of past events that has had In The Way participation.
This page was last updated on: 01/29/11.


Room for rent in King's Road, North Point - Spacious room near Fortress Hill MTR !!!
< > North Point flatshare > Spacious room near Fortress Hill MTR !!!
One cosy room is available in a 3 bedroom flat in Fortress Hill. Great for those of you who want to live near Wan Chai, CWB, but don't want to pay CWB and Wan Chai prices. 2-3 MTR stops away are not too far considering it takes 2 min to get from one stop to the other!
The flat is 600 sq ft net size and very big by HK standards. The flat is conveniently located near Fortress Hill MTR exit A, just 30 seconds walk, you just cross the street. Also there is a nice rooftop with seaview :) just a little extra bonus!
There is a huge park about 5-10 min walk from the flat, where you can unwind, jog and relax after a long day at work.
Kitchen, bathroom and living room are to be shared among flatmates. Kitchen features fridge, kettle, microwave oven, hotplate, toaster, kitchen accessories etc.
The middle bedroom features a double sized bed frame, built in wardrobe ...Price is 7000 HKD. Great for those budget minded, but who wanna get a taste of living on the Island side.
Internet is included. Bills are shared among the flatmates.


text:
Jack Garner: At the movies — and more
Jack Garner, Democrat and Chronicle
As an alternative, critic Jack Garner recommends:
DEADLINE U.S.A. This 1952 film, from the latter stages of Humphrey Bogart's career, is an exciting old-school newspaper drama. And it's just reissued on Blu-ray. Bogart plays a crusading editor whose newspaper is about to be sold from underneath him. But, even if it's true, the editor is determined to complete one major story — the exposure of a crime boss, played with intense authority by Martin Gabel. Though occasionally a bit overblown, the film is still entertaining, and has a sense of authority about the newspaper business in the pre-digital, pre-social media era. The direction by Richard Brooks is as gritty as you'd expect from the filmmaker who later made Blackboard Jungle, Elmer Gantry, In Cold Blood and Looking for Mr. Goodbar. Plus, of course, it's Bogart.
Director: Brooks.
Cast: Bogart, Gabel, and Ethel Barrymore.
Jack's rating: 9.
New on DVD this week: The Boss, Born to Be Blue, Criminal, Hardcore Henry, Sing Street, Barbershop 3: The Next Cut, River, I Am Wrath, The New World (criterion collection) and Deadline U.S.A.
Next week: The Lobster, Trader, Humpback Whales (IMAX), Invasion of the Body Snatchers (1978 version), Louder Than Bombs, The Mark of Zorro, The Blacklist: Season 3, The Knick: Second Season and Viral.


text:
VN Alexander, novelist
Press 1996-2014
Press 2015-present
Locus Amœnus, 2015
Trixie, 2010
Naked Singularity, 2003
Smoking Hopes, 1996
Science / Philosophy
Alexander selected to serve on Fulbright Specialist roster, 2018-2020
Victoria Alexander has been selected for a three-year term as a Fulbright Specialist, available to serve institutions in over 150 countries worldwide. Alexander is an expert in Vladimir Nabokov's non-gradualist approach to the evolution of insect mimicry.
"As the number of students interested in arts and humanities programs declines worldwide, my work has focused on showing how these disciplines are vital to developing critical and creative thinking skills. My specialty, biosemiotics (the study of signaling and sign-use in living systems), combines the fields of poetics, complexity science, philosophy of language, aesthetics, and biology to investigate the nature of creativity, adaptation, learning, and intentionality."
The Fulbright Specialist program is supported by the U.S. Department of State's Bureau of Educational and Cultural Affairs (ECA) and World Learning, Non-US institutions interested in hosting Dr. Alexander can apply at https://fulbrightspecialist.worldlearning.org/eligibility-host-institutions/
This entry was posted in --biosemiotics, secularism, teleology, Uncategorized on August 18, 2018 by VN Alexander.
← Terrordise, semi-finalist in Austin Revolution Film Fest Free Range Humans: What Makes Good Government? →
Victoria N. Alexander, Ph.D., is a literary fiction novelist, writing about censored and controversial subjects with audacity, humor, and compassion. Her honors include the Washington Prize for Fiction (Smoking Hopes) Dallas Observer's "Best of 2003" (Naked Singularity) and the Literary Fiction Book Review award (Locus Amoenus). Her latest novel, Locus Amoenus, was also a Dayton Literary Peace Prize nominee. Her fiction is published by The Permanent Press. She is the editor of Dactyl Review and is currently working on a collection of short stories called Chance that Mimics Choice.
Alexander is also a philosopher of science, author of The Biologist's Mistress: Rethinking Self-Organization in Art, Literature and Nature. She is a Rockefeller Foundation Bellagio Center alum, former Public Scholar for the New York Council for the Humanities. She serves on the editorial boards of Biosemiotics journal (Springer Publishing) and Meaning Systems book series (Fordham University Press). Her work in saltational evolutionary theory appears in Fine Lines: Nabokov's Scientific Art, published by Yale University Press, which has received much praise from major international publications. She will be at the Digital Humanities Lab at ITMO University in St Petersburg, Russia on a Fulbright grant beginning in 2020. See full CV.
Strange Recital podcast features Chapter One of Locus Amoenus
Hamlet Blues by Ben Jörgensen
A brief summary of my research project in Russia
Chance the Mimics Choice published in Pangyus
On St Petersburg, isolation and connection
Meno's Stories on the Strange Recital Podcast
Fine Lines wins Nabokov Society Brian Boyd Prize
Who Owns the World? Co-operative Book Publishing
What is Biosemiotics?
Terrordise, a finalist Filmmatic Comedy Screenplay competition
2015 Press: reviews / interviews / features
–biosemiotics
Locus Amœnus, 2015 Audiobook
excerpt from Locus Amoenus
VN Alexander, Fulbright Specialist, available for art/science workshops
VNA: alexander (at) dactyl (dot) org
publisher: info (at) thepermanentpress (dot) com


Living Room Decorating Ideas You'll Love. These design ideas will help you transform your living room into a cozy retreat..An elk antler trophy is the focal point in this living room, and the palm tree triptych and a blue, green, and mulberry palette create a comfortable environment..Get living room decorating ideas to help spark your own unique living room redecoration projects. Check out our living room ideas and get inspired today! Ethan Allen.Your living room is one of the most lived in rooms in your home. To make it the best it can be, House Beautiful has pulled together inspiration and ideas from more than living rooms we love..


text:
Short summary - Sentimental Education
In the fall of 1840, eighteen-year-old Frederic Moreau was returning by steamer to his hometown of Nogent-on-Seine. He had already received his bachelor's degree and was soon to go to Paris to study law. Dreamy, scientific and artistic, "he found that the happiness that the perfection of his soul deserves lingered." On the boat, he met the Arnu family. The husband was a gregarious fellow of about forty and owned the Art Industry, an enterprise that connected a newspaper devoted to painting and a shop selling paintings. His wife, Maria, struck Frederick with her unusual beauty. "It was as if a vision appeared to him ... He had never seen such a delightful dark skin, such an enchanting body, such thin fingers." He fell in love with Madame Arnoux with a romantic and at the same time passionate love, not yet knowing what it was for life.
At Nogent, he met Charles Delorier, his college buddy. Due to poverty, Charles was forced to interrupt his education and serve as a clerk in the province. Both friends were going to live together in Paris. But so far only Frederick had funds for this, whom his mother lent. In college, friends dreamed of great deeds. Frederic is about becoming a famous writer, Charles is about creating a new philosophical system. Now he predicted an imminent revolution and regretted that poverty was preventing him from deploying propaganda.
Having settled in Paris, Frederic went through a set of ordinary secular entertainments, made new acquaintances and soon "fell into complete idleness." True, he wrote a novel in the spirit of Walter Scott, where he himself was the hero, and Madame Arnoux was the heroine, but this occupation did not inspire him for long. After several unsuccessful attempts, chance helped him enter Arn's house. Located in Montmartre, the Art Industries was something of a political and artistic salon. But for Frederick, the main thing was his insane love for Madame Arnoux, to whom he was afraid to confess his feelings. Delorier, who had already arrived in Paris by this time, did not understand his friend's hobbies and advised him to achieve his goal or to throw the passion out of his head. He shared a shelter with Frederick, lived on his money, but could not overcome the envy of his friend - the darling of fate. He himself dreamed of big politics, of leading the masses, reaching out to the socialists who were in their youth company.
Time passed, and both friends defended their dissertations, and Charles with brilliance. Frederick's mother could no longer send her son the necessary amount, besides, she was getting old and complained of loneliness. The young man had to leave the capital, with which all his affections and hopes were connected, and get a job in Nogent. Gradually he "got used to the province, plunged into it, and even his very love acquired a drowsy charm." At this time, Louise Rock, a neighbor's teenage girl, became Frederick's only joy. Her father was the manager of a large Parisian banker, Damrez, and successfully increased his own capital. Three more years passed in this way. Finally, an elderly uncle Frederick died, and the hero became the heir to a considerable fortune. Now he was able to return to Paris again, promising his mother to make a diplomatic career there. He himself, first of all, thought of Madame Arnoux.
In Paris, it turned out that Arnoux had already a second child, that the "Art Industry" began to bring losses and had to be sold, and in exchange to start trading in faience. Madame Arnoux, as before, did not give Frederick any hope of reciprocity. The hero was not pleased with the meeting with Delorier. He did not have a career as a lawyer, he lost several cases in court and now he too clearly wanted to join the inheritance of a friend and spoke too evil about people in some position. Frederick settled in a cozy mansion, finishing it in the latest fashion. Now he was wealthy enough to enter the capital's elite circles. However, he still loved old friends, some of whom were completely indigent - for example, the eternal loser, the ardent socialist Senecal or the republican Dussardier - honest and kind, but somewhat limited.
Frederick was by nature soft, romantic, delicate, he was not very prudent and sometimes he was really generous. Not devoid of ambition, he nevertheless could not choose a worthy use for his mind and abilities. Now he took up literary work, then for historical research, then studied painting, then pondered a ministerial career. He did not complete anything. He found an explanation in his unhappy love, which paralyzed his will, but he could not resist the circumstances. Gradually, he became more and more close to the Arnu family, became the closest person in their house, constantly communicated with her husband and knew everything about his secret adventures and financial affairs, but this only added to his suffering. He saw that the woman adored by him endures the deception of not devoid of charm, but a vulgar and ordinary businessman, such as Jacques Arnoux, and for the sake of the children keeps her husband faithful.
Heart melancholy, however, did not prevent the hero from leading a secular life. He attended balls, masquerades, theaters, trendy restaurants and salons. He entered the house of the courtesan Rosanette, nicknamed the Captain, Arnu's mistress, and at the same time became a regular with the Damrezes and enjoyed the favor of the banker herself. Delorier, who was still forced to settle for thirty sous dinners and work the day, was angry at his friend's absent-minded life. Charles dreamed of his own newspaper as the last chance to gain an influential position. And one day he directly asked Frederick for money. And although he needed to withdraw a large amount from the capital stock, he did it. But on the last day he took fifteen thousand francs not to Charles, but to Jacques Arnoux, who was threatened with trial after an unsuccessful deal. He saved his beloved woman from ruin, feeling guilty before a friend.
There was confusion in society on the eve of the revolution, and so did Frederick's feelings. He still reverently loved Madame Arnu, but at the same time he wanted to become Rosanette's lover. "Communication with these two women was like two melodies; one was playful, impetuous, amusing, while the other was solemn, almost prayerful. " And at times Frederic dreamed of a connection with Madame Damrez, which would give him weight in society. He was a child of light - and at the same time he already managed to feel the coldness and falsity of his brilliance.
Having received a letter from his mother, he again left for Nogent. Neighbor Louise Rock by that time had become a rich bride. She loved Frederick from adolescence. Their marriage was, as it were, tacitly resolved, and yet the hero hesitated. He returned to Paris again, promising the girl that he would not leave for long. But a new meeting with Madame Arnoux canceled all plans. Rumors of Frederick's plans reached her, and she was shocked by this. She realized that she loved him. Now he denied everything - and the passion for Rosanette, and an early marriage. He swore eternal love to her - and then for the first time she allowed him to kiss her. They actually confessed their love for each other and for some time met as true friends, experienced quiet happiness. But they were not destined to get close. Once Madame Arnoux had already agreed to meet with him, but Frederic waited in vain for her for several hours. He did not know that Mrs. Arnu's little son fell seriously ill at night and she took it as a sign of God. Out of anger, he brought Rosanette to specially rented rooms. It was a February night in 1848.
They were awakened by gunfire. Out on the Champs Elysees, Frederick learned that the king had fled and a republic was proclaimed. The Tuileries doors were open. "Everyone was seized by a frantic joy, as if the vanished throne had already given way to boundless future happiness." The magnetism of the enthusiastic crowd passed on to Frederick. He wrote an enthusiastic article for the newspaper - a lyrical ode to the revolution, together with his friends began to go to workers' clubs and rallies. Delorier begged from the new authorities to appoint a commissar to the province. Frederick tried to run for the Legislative Assembly, but was booed as an aristocrat.
In secular circles, there was a rapid change in political sympathies. Everyone immediately declared themselves supporters of the republic - from the frivolous Captainess to the Council of State, the Damrezes and the Archbishop of Paris. In fact, the nobility and the bourgeois were only worried about the preservation of their usual way of life and property. The proclamation of the republic did not solve the problems of the lower classes. In June, a workers' rebellion began.
At this time, Frederic, already cooled to politics, was experiencing something like a honeymoon with Rosanette. She was flighty, but natural and spontaneous. In Paris, barricades were built, shots rang out, and they left the city, lived in a rural hotel, wandered through the woods all day or lay on the grass. Political unrest "seemed to him insignificant in comparison with their love and eternal nature." However, having learned from the newspaper about the injury of Dussardier, Frederic rushed to Paris and again found himself in the thick of things. He saw how the uprising was ruthlessly suppressed by the soldiers. "With triumph, stupid, bestial equality has declared itself; the same level of bloody meanness was established, the aristocracy raged in the same way as the rabble ... the public mind became clouded. " Inveterate liberals have now turned into conservatives, and radicals have found themselves behind bars - for example, Senecal.
These days Louise Rock, dying of anxiety for her lover, came to Paris. She did not find Frederick, who lived with Rosanette in another apartment, and only met him at a dinner at the Damrezes'. Among the ladies of the world, the girl seemed to him provincial, he spoke to her evasively, and she bitterly realized that their marriage was canceled.
Delorier's commissioner career ended ingloriously. "Since he preached brotherhood to the conservatives, and respect for the law to the socialists, some shot at him, while others brought a rope to hang him ... He knocked on the doors of democracy, offering to serve it with a pen, speech, his activities, but everywhere was rejected ... "
Rosanette gave birth to a child, but he soon died. Frederick gradually cooled to her. Now he is having an affair with Madame Damrez. He deceived both, but in return their love for him only grew stronger. And Madame Arnoux always lived in his thoughts. When the banker Damrez - one of the largest bribe-takers of his time - died of illness, the widow over her husband's coffin herself proposed to Frederick to marry her. He understood that this marriage would open up many opportunities for him. But this wedding was not destined to come true. Again it took money to save Arnu from prison. Frederick borrowed them from the new bride, naturally, not to mention the purpose. She found out and decided to take revenge with her usual cunning. Through Delorier, she used old promissory notes and obtained an inventory of Arnoux's property. And I also came to the auction when things were going under the hammer. And in front of Frederick's eyes, despite his desperate request, she bought a trinket, with which he had dear memories. Immediately after that, Frederic broke up with her forever. He also broke with the Captain, who truly loved him.
The unrest in Paris continued, and one day he accidentally witnessed a street brawl. Before his eyes, he was killed by a policeman - with a cry "Long live the republic!" - Dussardier. "The policeman looked around, looked around everyone, and the stunned Frederic recognized Senecal ..."
... Frederic traveled, had more than one romance, but never married, and "the acuteness of passion, all the charm of feeling were lost. Years passed, he put up with this idleness of thought, sluggishness of the heart. " Twenty years later, he saw again Madame Arnu, who now lived in the province. It was a sad meeting of old friends. Frederic also met with Delorier. He at one time married Louise Rock, but soon she ran away from him with some singer. Both friends now led the humble life of respectable bourgeois. Both were indifferent to politics. Summing up their lives, they admitted that "both of them did not succeed - both the one who dreamed of love and the one who dreamed of power."


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

Filamentary structures in the interstellar medium (ISM) have long been recognized \citep[e.g.,][]{sch79} but
their role in the process of star formation has received focused attention
only recently thanks to long-wavelength Herschel data \citep[e.g.,][]{mol10,and10}. With these data, recent
studies have demonstrated the ubiquity of the filaments in the cold ISM of our Milky Way \citep[e.g.,][]{mol10,and10,stu15,stu18a}.
Meanwhile, analysis of Herschel data has revealed a close connection
between filamentary clouds and star formation \citep[e.g.,][]{and10,and14,kon15,stu15,stu16,liu18}.  For instance,
most cores are detected in filamentary clouds \citep{and14,kon15,stu15}.
Moreover, with gas velocity information, protostellar cores are found kinematically coupled to the dense filamentary
environments in Orion \citep{stu16}; that is, the protostellar cores have similar radial velocities as the gas filament.

The overarching goal of obtaining empirical observational information of the physical state of observed filaments
has radically improved with the gradual availability and subsequent exploitation of gas radial velocities, which
reveal internal kinematics of the filaments in great detail \citep[e.g.,][]{hac11,tac14,hen14,beu15,taf15, hac17,hac18, lux18}.
Indeed, the kinematics is the only way to probe not only where the mass is presently, but also most importantly how it is moving under the influence of various possible forces.  In short, the gas kinematics provide a powerful window into the physical processes at play in the conversion of gas mass into stellar mass in filaments.
Velocity gradients have been for example interpreted as being driven by gravity \citep[e.g.,][]{hac11,tac14, hen16c, wil18, lux18, yua18}. For instance,
velocity gradients along the filament
may be related to longitudinal collapse leading to core formation \citep[e.g.,][]{hac11,kir13,per13,per14, tac14, hac17, wil18,lux18}, or those perpendicular to the filament
may result from the filament rotation or radial collapse \citep[e.g.,][]{rag12,kir13,beu15,wug18,liu18b}.

With the goal of understanding the link between dense cores and star formation  in filamentary clouds, we have investigated
the filamentary cloud G350.54$+$0.69 (hereafter G350.5) using {\it Herschel} continuum data (see Fig.\,1 of \citealt{liu18}, hereafter Paper\,I). G350.5\ is a straight and isolated
in morphology and composed of two distinct filaments, G350.5-N\ in the north and G350.5-S\ in the south. G350.5-N(S) is $\sim 5.9$\,pc ($\sim 2.3$\,pc) long with a mass of
$\sim 810$\,$M_{\odot}$~($\sim 110$\,$M_{\odot}$). The nine gravitationally bound dense cores associated with low-mass protostars suggest
 a site of ongoing low-mass star formation. In this work, we shift the focus to the gas kinematic properties. The nature of its simple morphology would be helpful in reducing the velocity ambiguities resulting from projection effects of potentially complex morphologies.

This paper is organized as follows: observations are described in Section\,2,  analysis results are presented
in Section\,3, the discussion is given in Section\,4 to a large-scale periodic velocity fluctuation along the main structure of the filament G350.5,
and a summary is put in Section\,5.

\section{Observations}
Observations of $^{13}$CO, and C$^{18}$O~(2-1) toward G350.5\ were made simultaneously using the Atacama Pathfinder Experiment
(APEX\footnote{This publication is based on data acquired with the Atacama Pathfinder Experiment (APEX). APEX is a collaboration between the Max-Planck-Institut fur Radioastronomie, the European Southern Observatory, and the Onsala Space Observatory. }) 12--m telescope \citep{gus06} at Llano de Chajnantor (Chilean Andes) in the on-the-fly mode on September 24, 2017.
The observations were centered at $\alpha_{2000}=17^{\mathrm{h}}18^{\mathrm{m}}13\fs84,\ \delta_{2000}=-36\degr28\arcmin21\farcs5$\ with a mapping size of $15\arcmin\times16\arcmin$, rotated by $50\degr$ relative to
the RA decreasing direction.
An  effective spectral resolution of 114\,KHz or 0.15\,km\,s$^{-1}$\ is reached at a tuned central frequency of 220\,GHz between
both for $^{13}$CO~(2-1) and for C$^{18}$O~(2-1).
The angular resolution at this frequency is $\sim 28\arcsec$,  which corresponds to $\sim 0.2$\,pc at the distance of G350.5, $1.38\pm0.34$\,pc (see Paper\,I). The reduced spectra finally present a typical rms value of 0.42\,K. More details on the
data reduction can be found in Paper\,I.

\section{Results}
\label{sec:result}
\subsection{Spatial distribution of the gas filament}
\label{sec:gas:distr}
\begin{figure}
\centering
\includegraphics[width=3.4 in]{G350_COaver.pdf}
\caption{Average spectra of $^{13}$CO, and C$^{18}$O~(2-1) over the G350.5\ filamentary cloud. The black color stands for the observed spectrum.
The red line is the Gaussian fitting to the spectrum of $^{13}$CO, which is a sum of the two Gaussian components (blue lines), the weak-emission one from $-9.0$ to
$5.7$\,km\,s$^{-1}$, and the  major one from $-5.7$ to $-2$\,km\,s$^{-1}$. The green line is the single-component Gaussian fitting to the spectrum of C$^{18}$O, which matches the major
component of the $^{13}$CO\ spectrum. The vertical dashed black line represents a systematic velocity of $-3.9$\,km\,s$^{-1}$.
}
\label{fig-spec_aver}
\end{figure}

Before addressing the kinematic structure of G350.5, we first describe the spatial distribution of molecular emission.
Figure\,\ref{fig-spec_aver} presents the average spectra of $^{13}$CO, and C$^{18}$O~(2-1) over the whole G350.5\ system.
The $^{13}$CO\ profile has two velocity components, one from $-9.0$ to
$5.7$\,km\,s$^{-1}$\ (hereafter weak-emission component) and the other from $-5.7$ to $-2$\,km\,s$^{-1}$\ (hereafter major component);
C$^{18}$O\ has a single-peak profile corresponding to the major component of $^{13}$CO.
The systemic velocity is determined to be  $-3.9$\,km\,s$^{-1}$\ from the average spectrum of C$^{18}$O~(2-1).

\begin{figure*}
\centering
  \includegraphics[width=6.8 in]{G350_gas_emission.pdf}

\caption{(a--b:) Velocity-integrated intensity maps of the two velocity components of $^{13}$CO~(2-1) toward G350.5, the major one from $-5.7$~to~$-2$\,km\,s$^{-1}$, and the weak-emission one
from $-9$~to~$-5.7$\,km\,s$^{-1}$.  (c:) Velocity-integrated intensity of C$^{18}$O~(2-1), integrated over $-7$ to $-1$\,km\,s$^{-1}$.  The pixel size of the three maps is reduced to 7$\arcsec$, a quarter of the beam size, for a better visualization.  The cyan curves in all panels represent the spines of the two discontinuous filaments as identified in Paper\,I and the black contours stand for the $N_{\rm H_2}$ column density (see Paper\,I), starting from $1.8\times10^{22}$\,cm$^{-2}$\ with a step of $0.6\times10^{22}$\,cm$^{-2}$\ ($\sigma=0.04\times10^{22}$\,cm$^{-2}$).
}
\label{fig-13CO_emission}
\end{figure*}

Figure\,\ref{fig-13CO_emission} shows the velocity-integrated intensity maps of  $^{13}$CO, and C$^{18}$O~(2-1). The spatial distribution of the major component of $^{13}$CO\ (see Fig.\,\ref{fig-13CO_emission}a) matches the column density (\ensuremath{N_{\mathrm{H_{2}}}}) distribution (black contours, derived from Herschel data in Paper\,I through the pixel-wise spectral energy distribution fitting, e.g., \citealt{liu16,liu17}), showing two discontinuous filaments as indicated by the two cyan curves.
 In addition, some small-scale structures (i.e., filament `branches') stretch perpendicular to the main structure of the cloud G350.5, which
coincide with the perpendicular dust striations surrounding the filament as observed in Herschel continuum
images (see Paper\,I).  Emission of the major component of $^{13}$CO~(2-1) has a C$^{18}$O\ counterpart  (in Fig.\,\ref{fig-13CO_emission}c), but the latter is more narrowly distributed than the former.
In contrast, the weak-emission component of $^{13}$CO~(2-1) in Fig.\,\ref{fig-13CO_emission}b has no detectable C$^{18}$O\ counterpart. However, it can be seen that the two components of  $^{13}$CO\ are indeed associated with each other. In the south and center of the filament, the two most prominent clumps in the intensity map of the $^{13}$CO\ weak-emission component can also be found in that of the major component. This is supportive of the association between the weak-emission and major components.

\subsection{Velocity field along the filament}
\label{sec:vel:cent}
\begin{figure}
\centering
\includegraphics[width=3.4 in]{G350vel_centroid_C18O_orig.pdf}
\caption{Velocity centroid map of C$^{18}$O~(2-1) for the filamentary cloud G350.5. Only the main filament is shown
because of sufficient detection of C$^{18}$O~(2-1) therein. The pixel size of the map is 14$\arcsec$, half of the beam size, as recommended by the APEX observatory.
All pixels correspond to detection greater than  $3\sigma$ (i.e., $\sigma=0.4$\,K\,km\,s$^{-1}$).
The red and blue color scales can be regarded as the red and blue-shifted velocities with respect to
the systematic velocity $-3.9$\,km\,s$^{-1}$.  A large-scale periodic velocity fluctuation appears almost
along the main structure. The black contours represent the $N_{\rm H_2}$ column density, starting from
$1.8\times10^{22}$\,cm$^{-2}$\ with a step of $0.6\times10^{22}$\,cm$^{-2}$.
The dense cores identified in Paper\,I are also labelled as C1--C8.
}
\label{fig-C18O_emission_vel}
\end{figure}

To investigate the large-scale kinematics, we show  the velocity centroid map of C$^{18}$O~(2-1) of the cloud G350.5\ in Fig.\,\ref{fig-C18O_emission_vel}.
Velocity information is shown only in the main structure of the filament, beyond which C$^{18}$O~(2-1) emission is too noisy ($<2\sigma$), overlaid with
the \ensuremath{N_{\mathrm{H_{2}}}}\ contours (Paper\,I) for comparison. Strikingly, a large-scale periodic velocity fluctuation appears along the main structure, which is $\sim8$\,pc long (Paper\,I).
The nature of the large-scale and periodic signal suggests that the observed velocity fluctuation is real, otherwise, this periodicity will be hardly maintained on a large scale if it happens by chance.
Specifically,  the red and blue colors in Fig.\,\ref{fig-C18O_emission_vel} represent the red and
blue-shifted velocities relative to the systemic velocity of $-3.9$\,km\,s$^{-1}$. Comparing the \ensuremath{N_{\mathrm{H_{2}}}}\ contours with the velocity centroid map,
we find a spatial correspondence between the velocity extremes and the density enhancements for some dense cores (i.e., C2, C5, C6, C7a,b, and C8).
The possible origins of this correspondence will be discussed
further in Sect.\,\ref{sec:disc}. We do not present here the velocity centroid map of $^{13}$CO~(2-1), which does not show the periodic fluctuation as in C$^{18}$O~(2-1) emission.
Since $^{13}$CO\ tends to trace more extended emission than C$^{18}$O, the velocity characteristics revealed by both species are not necessarily the same.

\subsection{Velocity dispersion along the filament measured from both $^{13}$CO\ and C$^{18}$O}
\begin{figure*}
\centering
\includegraphics[width=3.4 in]{G350_vel_disp_bothAB_uncorr.pdf}
\includegraphics[width=3.4 in]{G350_vel_disp_bothAB.pdf}
\caption{Histogram of the total velocity dispersion measured from both $^{13}$CO\ (red) and C$^{18}$O~(2-1) (blue) for G350.5. In panel\,(a) is the observed velocity dispersion.
The mean values in the observed velocity dispersions measured from  $^{13}$CO\ and C$^{18}$O\ are $2.9\pm0.4\,\sigma_{\rm th}$ (red dashed line),
and $2.0\pm0.3\,\sigma_{\rm th}$ (blue dashed line), respectively.
In panel\,(b) is the opacity-corrected (intrinsic) velocity dispersion. The mean values are $2.1\pm0.2\,\sigma_{\rm th}$ from $^{13}$CO\ (red dashed line),
and  $1.9\pm0.3\,\sigma_{\rm th}$ from C$^{18}$O\ (blue dashed line).
The different distributions of the velocity dispersions of $^{13}$CO\ before and after the opacity correction demonstrate that the line opacity can cause the broadening of
the intrinsic velocity dispersion. The intrinsic velocity dispersion distributions indicate that the  overall turbulent motions of the filament G350.5 are supersonic (i.e., the 3D Mach
number follows $M_{3D} >2$).
}
\label{fig-vel_disp}
\end{figure*}

The observed velocity dispersion ($\sigma_{\rm obs}$) is measured from both $^{13}$CO\ and C$^{18}$O~(2-1) in
the main structure of the filament where both species are well-detected. In principle, $\sigma_{\rm obs}$
can be estimated from the second-order moment of the PPV data cube. However, this method will cause additional uncertainties due to the simple treatment of
multiple-velocity components as one. To better estimate $\sigma_{\rm obs}$ especially from $^{13}$CO~2-1, we define 47 positions along the ridgeline of the filament, 41 in G350.5-N\ and 6 in G350.5-S.
Neighbour positions are separated by one pixel, half of the beam size of both $^{13}$CO\ and C$^{18}$O\ maps.
$\sigma_{\rm obs}$ is then obtained from the Gaussian fitting to the spectra of both $^{13}$CO, and C$^{18}$O~(2-1) at the selected 47 positions.
The fitting plots are shown in Fig.\,\ref{fig-guassA}.

The velocity dispersion combines the contributions from both thermal and non-thermal gas motions in turbulent clouds. However, their contributions can be overestimated due to the line broadening
by optical depth.  Such overestimate can be expressed analytically as a function of the optical depth \citep{phi79}:
\begin{equation}\label{eq:broad}
\sigma_{\rm obs} =\frac{1}{\sqrt{ln 2}}\left[ln \left( \frac{\tau}{ln\left(\frac{2}{e^{-\tau}+1} \right) } \right) \right]^{1/2} \sigma_{\rm int},
\end{equation}
where $\sigma_{\rm int}$ is the intrinsic velocity dispersion unaffected by optical depth $\tau$ (see Appendix\,\ref{sec:opt:dep}).
For comparison, we calculate the gas dispersions (i.e., non-thermal dispersion $\sigma_{\rm NT}$, and the total dispersion $\sigma_{\rm tot}$)  based on the observed, and intrinsic velocity dispersions measured from both $^{13}$CO\ and C$^{18}$O, respectively, as follows:
\begin{equation}\label{eq:vel:disp}
\begin{array}{rrr}
\sigma_{\rm NT} = \sqrt{\sigma_{\rm obs/int}^2-\frac{kT_{\rm k}}{m}}, \\
\sigma_{\rm th} = \sqrt{\frac{kT_{\rm k}}{ \mu_p m_{\rm H} }}, \\
\sigma_{\rm tot} = \sqrt{\sigma_{\rm NT}^2+\sigma_{\rm th}^2}, \\
\end{array}
\end{equation}
where $\sigma_{\rm obs/int}$ can be replaced either with $\sigma_{\rm obs}$ or with $\sigma_{\rm int}$ (see Eq.\,\ref{eq:broad}), $k$ is  Boltzmann's constant, $T_{\rm k}$ is the gas kinetic temperature, $m$ is the mass of the
two species,  $m_{\rm H}$ is the mass of atomic hydrogen, and $\mu_p=2.33$ is the mean molecular weight per free particle for an abundance ratio
$N(H)/N(He)=10$ and a negligible admixture of metals (e.g., \citealt{kau08}).
The gas kinetic temperature here was assumed to be equal to the average dust temperature ($T_{\rm d} \sim18 \,K$) of the filament instead of the excitation temperature of
each species since the latter is found to be $\sim6$\,K on average lower than the former, indicating that the two species might
not be fully thermalized in the filament (see Appendix\,\ref{sec:ex:temp} for the calculation of the excitation temperature).
The assumed $T_{\rm k}$ gives rise to the thermal sound speed  of molecular gas $\sigma_{\rm th}\sim0.25$\,km\,s$^{-1}$.

Figure\,\ref{fig-vel_disp} presents the histograms of both the observed ($\sigma_{\rm tot,obs}$ in panel a) and intrinsic ($\sigma_{\rm tot,int}$ in panel b) total dispersions of gas
for the entire filament represented by 41 positions in G350.5-N\ and 6 in G350.5-S. The intrinsic gas dispersion is overall smaller than the observed one without the optical-depth correction, indicating that the optical depth correction is important, especially for $^{13}$CO.   In view of this, we analyse only the intrinsic gas dispersion (in Fig.\,\ref{fig-vel_disp}b) in what follows.
The average total dispersions are $2.1\pm0.2\,\sigma_{\rm th}$, and $1.9\pm0.3\,\sigma_{\rm th}$, measured from $^{13}$CO, and C$^{18}$O, respectively.
These values indicate that the
filament G350.5\ as a whole is supersonic with a mach number of $M_{3D} > 2$ (see Fig.\,\ref{fig-vel_disp}b), where
the 3D Mach number is $M_{3D}= \sqrt{3} \sigma_{\rm NT,int}/\sigma_{\rm th}$ given the 1D measurement $\sigma_{\rm NT,int}$, and assuming isotropic turbulence
 in three dimensions \citep[e.g.,][]{kai17b}.

\subsection{Virial analysis along the filament}
\label{sec:vel_fluct}
\begin{figure*}
\centering
\includegraphics[width=3.2 in]{G350_energy_compA_v2.pdf}
\includegraphics[width=3.2 in]{G350_energy_compB_v2.pdf}
\caption{Virial analysis through the comparisons between turbulent ($T$), magnetic energies ($M$) and gravitational potential ($W$) for G350.5-N\ (in panel\,a), and
for G350.5-S\ (in panel\,b).  Several peaks are related to dense cores (also see Fig.\,\ref{fig-C18O_emission_vel}) as indicated by vertical lines. The comparison shows that
the gravity dominates over both turbulence and magnetic fields, and is a major driver to the global fragmentation of G350.5 from clouds to dense cores.
}
\label{fig-virial}
\end{figure*}
The complex interactions between turbulence, gravity and magnetic fields happen everywhere in  molecular clouds and regulate star formation therein.
We can describe these interactions  through the virial theorem.
According to \citet{fie00}, the virial equation of self-gravitating, magnetized turbulent filamentary clouds can be written in the form:
\begin{equation}\label{eq:luminosity}\label{eq:plummer}
2T_{\rm net}+W+M = 0.
\end{equation}
Therefore, the virial equilibrium  of the clouds depends on the competition between the net kinetic energy ($T_{\rm net}$), magnetic energy ($M$), and gravitational potential ($W$).
$T_{\rm net}$ accounts for the difference between the internal ($T_{\rm int}$) and external ($T_{\rm ext}$) turbulent energy, assuming that molecular clouds are confined by the external pressure rather than completely isolated. Note that all energies here are measured per unit length.

The internal kinetic energy $T_{\rm int}$ is calculated as:
\begin{equation}
T_{\rm int} = \frac{1}{2}\ M_{\rm line}\ \sigma^2_{\rm tot,int},
\end{equation}
where $M_{\rm line}$\ is the line mass along the filament, which can be obtained in Fig.\,3 of Paper\,I.
While $\sigma_{\rm tot,int}$ measured from $^{13}$CO\, and C$^{18}$O~(2-1) are similar,
the one from $^{13}$CO~(2-1) was finally adopted in the calculation since $^{13}$CO\ emission tends to trace larger-scale gas.
 The external turbulent energy $T_{\rm ext}$ can be expressed as a function of the external pressure $P_{\rm ext}$:
\begin{equation}
T_{\rm ext} =  {\it k} P_{\rm ext}\ \pi R_{\rm fil}^2,
\end{equation}
where {\it k} is the Boltzmann constant and $R_{\rm fil}$ is the filament radius, $\sim 0.5$\,pc as measured in Paper\,I. A conservative value of $P_{\rm ext}=5\times10^4$\,K\,cm$^{-3}$ is assumed,
which is in the range between $10^4$\,K\,cm$^{-3}$ for the general ISM \citep{chr89} and $10^5$\,K\,cm$^{-3}$ for several molecular clouds associated
with HI complexes \citep{bou90}.

The gravitational potential energy $W$ is derived from the line mass of the filament:
\begin{equation}
W = -M_{\rm line}^2 G,
\end{equation}
where $G$ is the gravitational constant.
The magnetic energy  $M$ is written as:
\begin{equation}
M = \frac{B^2}{2\mu_0} \pi R_{\rm fil}^2,
\end{equation}
where $B$ is the magnetic field strength and  ${\mu_0}$ is the permeability of free space.
$B$ is estimated following the empirical linear relationship between the field strength and
gas column density. This relationship was summarized by \citet{cru12} from Zeeman measurements in the form:
\begin{equation}\label{eq:luminosity}\label{eq:plummer}
B = C \times N_{H}\, 10^{-21}\,\mu G,
\end{equation}
where $C$ is a constant, and $N_{\rm H}$ is the column density of atomic hydrogen gas. This constant was given to be 3.8 by \citet{cru12} under the assumption of magnetic critical condition and a spherical shape of clouds, and improved to be 1.9 by \citet{li 14} assuming a sheet-like shape.
The mean column density of the cloud G350.5, $N_{\rm H_2} = 8\times10^{21}$\,cm$^{-2}$\ (Paper\,I), indicates
an average B-field of $16$\,$\mu$G. Even though this estimate of the B-field strength is very indirect, it can give us some insight into the role of the B-field versus gravity (see below).

Figure\,\ref{fig-virial} presents the comparison between turbulent ($T$), gravitational ($W$) and magnetic ($M$) energies per unit length along the main structure of
the two filaments G350.5-N, and G350.5-S.  It can be seen that $W$ (black curve) is greater than the sum of $T_{\rm net}$ and $M$ (light grey curve)
along the main structure of both G350.5-N\ and G350.5-S\ with respective mean ratios of $W/(T_{\rm net}+M)=2.0\pm1.6$, and $2.5\pm1.8$. This trend is in particular evident
for the dense cores which correspond to the peaks in the distributions (see Fig.\,\ref{fig-virial}). This suggests that gravity dominates over both turbulence and
 magnetic fields, and is a  major driver to the global fragmentation
of G350.5\ from clouds to dense cores. This is consistent with  our previous analysis (Paper\,I) showing that G350.5\ could have undergone radial collapse and
fragmentation into distinct small-scale dense cores. Moreover, one can see that only turbulence without the aid of the B-field is not able to counteract gravity, suggesting the critical role of B-field in regulating molecular clouds against gravity. This is in agreement with existing observations showing that magnetic fields are important in filamentary clouds  \citep[e.g.,][]{li 13,li 14,li 15, stu16, con16}. Future more accurate B-field strength measurements will provide direct constraints on the role of the magnetic fields in G350.5.

\section{Discussion: Large-scale velocity oscillations along the filament}
\label{sec:disc}
\begin{figure*}
\centering
\includegraphics[width=6.0 in]{G350_pv_NH2.pdf}
\caption{(a-b:) Velocity and column density distributions extracted along the spine of the filament G350.5-N.
(a): Position-velocity diagram of C$^{18}$O~(2-1). The detections greater than $3\sigma$ ($\sigma=0.42$\,K) are shown in grey-scale within the velocity channels from $-5.0$ to $-2.5$\,km\,s$^{-1}$.
The cyan crosses are the weighted average velocities by brightness temperatures, and fitted with  a sine function with a wavelength of $\sim 1.3$\,pc and an amplitude of $\sim 0.12$\,km\,s$^{-1}$. Literally, the blue
color curves stand for the blue-shifted velocities with respect to the systematic velocity of $-3.9$\,km\,s$^{-1}$, and the red ones for the red-shifted velocities.
(b:) Density distribution. Density peaks related to dense cores are indicated, i.e., C2 to C8, which are extracted from Fig.\,\ref{fig-C18O_emission_vel}. The velocity and column
density distributions do not show a good one-to-one correspondence between one another.
}
\label{fig-pvNH2}
\end{figure*}

\begin{figure*}
\centering
\includegraphics[width=7.0 in]{models.pdf}
\caption{(a:) schematic representation of GI-driven core formation along a filament, which is adapted from Fig.\,12 of \citet{hac11}.
Due to GI, the motions of core-forming gas converge towards the core centers where the density enhances
but the relative motions become static with respect to the systematic velocity. In this scenario, assuming that both  density ($\delta \rho$) and velocity ($\delta V$) follow sinusoidal distributions,
a $\lambda/4$ phase shift between them would be expected. (b): schematic representation of a physical oscillating filament (e.g., induced by an MHD wave). The filament moves toward and away from
an observer. In this scenario, the correspondence between the velocity extremes (i.e., red/blue-shifted velocities) and the density enhancements is expected if the filament (density) oscillates sinusoidally. The red and blue colors indicate the red, and blue-shifted velocities (motions) with respect to an observer. Note that  the physical intensities of $\delta \rho$ and $\delta V$ are ignored in the schematic demonstration.
}
\label{fig-models}
\end{figure*}

As mentioned in Sect.\,\ref{sec:vel:cent}, a large-scale periodic velocity oscillation is found  along the entire filament.
This oscillation feature may be related to kinematics of either core formation or a  large-scale oscillation
(e.g., wave-like perturbations triggered by material accretion flows onto the filament or  a standing wave \citet{stu18b}). In what follows, we will make an attempt to
investigate the nature of the observed large-scale velocity oscillation in G350.5-N. Since G350.5-S\ is disconnected to G350.5-N\ in Fig.\,\ref{fig-C18O_emission_vel} and G350.5-S\ itself has insufficient detection in the diffuse region, the nature
of the velocity field of G350.5-S\ requires detailed investigation with sensitive and higher-resolution observations. To better visualize the
velocity oscillation along G350.5-N, we make the position-velocity (PV) diagram shown in Fig.\,\ref{fig-pvNH2}a.
The color scale is the main-beam temperature with  at least $3\sigma$ ($\sigma=0.42$\,K) detection within $-5.0$ to $-2.5$\,km\,s$^{-1}$.

To highlight the velocity fluctuation feature, we calculate the average velocities weighted by the main-beam temperature, as shown in cyan crosses.
In Fig.\,\ref{fig-pvNH2}a, the velocity oscillation behaves periodically along the filament. Particularly, it can be fit  with a sine function with a  wavelength of $\sim 1.3$\,pc and an amplitude of $\sim 0.12$\,km\,s$^{-1}$.

\subsection{Core formation through longitudinal gravitational instability?}
\label{sec:core:form:grav:contr}

In Paper\,I, nine identified cores are found to be distributed almost periodically along the
entire filamentary cloud G350.5\ and the average projected separations between them are measured to be  $\sim 0.9$\,pc.
This separation is consistent with the prediction ($\sim 1.1$\,pc in Paper\,I)
by the ``sausage'' (\textbf{gravitational}) instability \citep{cha53,nag87}, and comparable to the wavelength of the periodic velocity signature
($\sim 1.32$\,pc, see above) inferred from the periodic velocity distribution as well. Therefore, the periodic velocity fluctuation may be
associated with the kinematics of filament fragmentation into cores through gravitational instability (GI hereafter).

Actually, this periodic-type velocity fluctuation was already predicted in the analytic models dedicated to GI-induced core formation
in a uniform, incompressible filament threaded by a purely poloidal magnetic field  \citep[e.g.,][]{cha53}.
In simulations, the GI is generally represented with
redistributions of the gas in the filament via motions that have a dominant velocity component parallel to the cylinder axis due to longitudinal
gravitational contraction at least during the first stages of evolution \citep[e.g.,][]{nak93,fie00b}. The gas redistribution processes can be summarized in
the schematic model of core formation as seen in Fig.\,\ref{fig-models}a, where the motions of core-forming gas converge towards the core center along the filament,
leading to the density enhancements peaking at a position of vanishing velocity. Assuming that both density and velocity
perturbations (oscillations) are sinusoidal (periodic), a $\lambda/4$ shift between them can be expected (\citealt{hac11} for
more details).  The similar pattern of velocity oscillation and its association with the density distribution have been reported in Taurus/L1517 \citep{hac11}.

Comparing with the scenario of GI-induced core formation models, we do not observe a $\lambda/4$ ($\sim 0.33$\,pc) phase shift between
the velocity and density distributions (see Fig.\,\ref{fig-pvNH2}).
In addition, the predicted vanishing of velocity (see above) is not observed in most of the density enhancements cores (i.e., C2, C5, C6, C7a,b, and C8),
and instead the velocity extremes coincide spatially with the density enhancements.
Note that the above-mentioned models are rather idealised, and only designed  for a straight filament. For example,
if a filament were randomly kinked/curved on small scales, neither the systematic phase shift between the velocity and density distributions or
the  vanishing of velocity at the position of cores would be expected in the core formation process (see scenario\,1 in Fig.\,12 of \citealt{hen14}).
However, we believe that the possibility of a randomly kinked structure is very low in G350.5-N\ since (random) small-scale kinks would not maintain a
large-scale coherent, periodic oscillation. On the other hand, a regular but oscillating geometry driven by some physical mechanism could be possible
(e.g., \citealt{gri17}, see model\,2 in Fig.\,\ref{fig-models}, and Sect.\,\ref{sec:mhd} for more discussions).

Moreover, upon inspection of  Fig.\,\ref{fig-C18O_emission_vel}, we can group all dense cores into six main mass-accumulation clumps, i.e.,
C1 [red], C2 [red], C3+4 [red], C5+6 [red+blue], C7a+b [red+blue], and C8 [red]. They are almost periodically separated, which is demonstrated to be
a result of filament fragmentation through GI (see above, and Paper\,I). Three of these clumps might have undergone further fragmentation
due to GI or Jeans collapse \citep[e.g.,][]{kai17}, leading to the observed multiplicity (i.e., from clumps to cores; C3+4 to C3 and C4, C5+6 to C5 and C6, and C7a+b to C7a and C7b).
Such clump-scale fragmentation may influence
the small-scale (inter-core) velocity distribution within the clumps. As a result, red and blue-shifted velocities would be expected on either side of dense cores in
a straight filament.  Assuming that G350.5-N\ is straight to some extent (see above), no red and blue-shifted velocities appearing on
either side of the dense cores within two of the three clumps (i.e., C5+6, and C7a+b), therefore, imply that
the clump-scale fragmentation (if any)  would not significantly affect  the large-scale periodic velocity pattern.

In addition, the average amplitude of the velocity oscillations is measured to be $\sim 0.12$\,km\,s$^{-1}$. This value is
 around three times greater than that observed in Taurus/L1517 \citep{hac11}. This difference could depend on the mass of
 dense cores and the inclination of the filament. Actually, the average mass of dense cores in G350.5-N\ is $\sim 20$\,$M_{\odot}$,
 around 10 times higher than that in Taurus/L1517. Assuming free-fall gas accretion onto dense cores along the filament, we roughly
calculate the infall velocity via the relation $V_{\rm infall} = \sqrt{GM*{\rm cos}\theta/r}$, where G is the gravitational constant, $r$ is the radius within which gas
flows onto dense cores, adopted to be $1/4\lambda$ (0.33\,pc), and $\theta$ is the inclination angle of the filament with respect to the line of sight.
As a result, the average mass $\sim 20$\,$M_{\odot}$\ yields $V_{\rm infall} = \sim 0.5$\,km\,s$^{-1}$\ for $\theta=0\degr$, and $\sim 0.4$\,km\,s$^{-1}$\ for $\theta=45\degr$,
both of which are around 4 times greater than the amplitude of the velocity oscillation in G350.5-N.
Note that these infall velocities  should be overestimated to be the accretion velocity of gas onto dense cores since neither
gas accretion is purely free-fall in reality nor the infall commences at an infinite radius as assumed in the above equation (e.g., \citealt{vaz19}).
Keeping this uncertainty in mind, and given
core formation through GI being at work in G350.5 (see above, and Paper\,I), we suggest that
core-forming gas motions induced by GI could contribute in part to the observed velocity oscillation.
  However, another mechanism (e.g., see Model\,2 in Fig.\,\ref{fig-models}, and Sect.\,\ref{sec:mhd}) is still required to explain
the discrepancy between the observations and idealized GI-induced core-formation models, i.e., the lack of a constant phase shift
observed between the velocity and density distributions.

\subsection{Large-scale MHD-transverse wave propagating along the filament?}
\label{sec:mhd}
As mentioned in Sect.\,\ref{sec:core:form:grav:contr}, there could be a mechanism responsible for the observed relation between the velocity and density distributions (see Fig.\,\ref{fig-pvNH2}).
We conjecture that this mechanism might be the MHD-transverse wave propagating along the filament, which can also produce a periodic velocity oscillation. Actually, this mechanism was reported both in observations and in simulations \citep[e.g.,][]{nak08,stu16}. For example,  combining both observed spatial and velocity undulations and the helical B-field measurements in the Orion integral-shaped filament (ISF),
\citet{stu16} suggested that repeated propagation of transverse waves through the filament are progressively digesting the material that formerly connected Orion A and B into stars in discrete episodes. In three-dimensional MHD simulations of star formation in turbulent, magnetized clouds, including feedback from protostellar outflows, \citet{nak08} mentioned that stellar feedback like outflows  can induce large-amplitude Alfv\'en waves, which perturb the
field lines in the envelope that thread other parts of the condensed sheet. The large Alfv\'en speed in the diffuse envelope allows different
parts of the sheet to interact with each other quickly. Such interaction can spring up global, magnetically mediated oscillations for the condensed material \citep{nak08}. The appearance of a large-scale MHD-transverse wave along the filament is understandable as long as there is a poloidal component of B-field, which is expected with generally helical and other configurations of 3D magnetic fields \citep[e.g.,][]{hei97,fie00,fie00b,stu16,sch18,rei18}

In the filament G350.5-N, the driving source of the large-scale MHD-transverse wave could result from outflows of young stellar objects \citep{nak08}. In addition,
the gas accretion flows onto the filament (see Paper\,I) could be an additional driving source.
 In principle, a wave-like shape of spatial density distribution could be expected as observed in the Orion-A ISF \citep{stu16}. However, it can not be recognized from Fig.\,\ref{fig-13CO_emission}. This could be because of projection effects. That is, the large-scale MHD-transverse wave oscillates toward and away from us (see model\,2 in Fig.\,\ref{fig-models}) while propagating along the filament. As a result, the filament is projected to be a rather straight morphology on the plane-of-sky but the periodic velocity oscillation can be observed to blue and red-shifted with respect to the systemic velocity.

To conclude, given the GI-induced core formation being at work in G350.5-N\ (see Sect.\,\ref{sec:core:form:grav:contr}), we suggest that
the observed periodic velocity oscillation may result from a combination of
the core-forming gas motions induced by GI
and a periodic physical oscillation driven by a MHD transverse wave. This combination can make $\lambda/4$ shift, as expected between the velocity and density distributions in the core-formation models (see Model\,1 of Fig.\,\ref{fig-models}), disappear due to the mixture of the two different motions.
Instead, the wave could cause the correspondence
between the velocity extremes and density enhancements  (see Fig.\,\ref{fig-pvNH2}) if the wave is stronger than the core-forming gas motions in velocity amplitude.
Despite of no definitive interpretation, it is worthwhile to test the possibility of the large-scale transverse wave being at work in G350.5-N. Therefore, we call for
future high sensitivity/resolution Zeeman, and dust polarization measurements to infer the B-field strength and to constrain the field morphology (see above).

\section{Conclusions}
We have analysed the internal kinematics of the filament G350.5\ with
our observations of $^{13}$CO, and C$^{18}$O~(2-1) by APEX. $^{13}$CO\ emission
reveals two clouds with different velocities. The major cloud G350.5\ corresponds
to $-5.7$ to $-2$\,km\,s$^{-1}$\ while the other one corresponds to  $-9.0$ to $5.7$\,km\,s$^{-1}$.
Our analysis shows
that the filament G350.5\ as a whole is supersonic and gravitationally bound.
In addition, we find a large-scale periodic velocity oscillation along the filament G350.5-N\ with a wavelength of $\sim 1.3$\,pc and an amplitude of $\sim 0.12$\,km\,s$^{-1}$. Comparing with the gravitational-instability induced core formation models, we suggest that
the observed periodic velocity oscillation may result from a combination of the kinematics of gravitational instability-induced core formation and a periodic physical oscillation driven by a MHD transverse wave. To test the latter, future high sensitivity, and resolution Zeeman, and dust polarization measurements toward G350.5\ are required to infer the B-field strength and to constrain the field morphology

\medskip
\noindent{\textbf{Acknowledgments}}\\
We thank the anonymous referee for constructive comments that improved the quality of our paper.
This work was in part sponsored by the Chinese Academy of Sciences (CAS), through a grant to
the CAS South America Center for Astronomy (CASSACA) in Santiago, Chile.
  AS acknowledges funding through Fondecyt regular (project code
1180350), ``Concurso Proyectos Internacionales de Investigaci\'on''
(project code PII20150171), and Chilean Centro de Excelencia en
Astrof\'isica y Tecnolog\'ias Afines (CATA) BASAL grant AFB-170002.  J. Yuan is supported by the National Natural Science Foundation of China
through grants 11503035, 11573036.
 This research made use of Astropy,
a community-developed core Python package for Astronomy (Astropy
Collaboration, 2018).

\bibliographystyle{mnras}

redpajama_set_name: RedPajamaArXiv


text:
53,148 Stanford California Premium High Res Photos
Browse 53,148 stanford california stock photos and images available or start a new search to explore more stock photos and images.
hoover tower, stanford university 7 - stanford california stock pictures, royalty-free photos & images
stanford university at dawn - stanford california stock pictures, royalty-free photos & images
students walk along covered footpath at stanford university - stanford california stock pictures, royalty-free photos & images
Person walks past archways during a quiet morning at Stanford University on March 9, 2020 in Stanford, California. Stanford University announced that...
Cyclists ride by Hoover Tower on the Stanford University campus on March 12, 2019 in Stanford, California. More than 40 people, including actresses...
Stanford University's Hoover Tower rises above the Stanford campus with the foothills of California's Santa Cruz Mountains in the distance. The Dish,...
John Elway of the Stanford Cardinal warms up before the Big Game against the California Golden Bears played on November 20, 1982 at Memorial Stadium...
art illustration map,palo alto city of san francisco bay area - stanford california stock illustrations
Hoover Tower looms during a quiet morning at Stanford University on March 9, 2020 in Stanford, California. Stanford University announced that classes...
Rabbit runs on the field during an NCAA Pac-12 football game between the Stanford Cardinal and the University of Oregon Ducks on October 14, 2017 at...
stanford university - stanford california stock pictures, royalty-free photos & images
Empty chairs and tables sit outside the usually bustling student union during a quiet morning at Stanford University on March 9, 2020 in Stanford,...
Smoke from the Camp Fire hangs over the Stanford University campus before the game between the Stanford Cardinal and the Oregon State Beavers at...
ilustration of stanford university art map.ca,usa - stanford california stock illustrations
John Elway of Stanford, , plays here in a game against San Jose State at Stanford Stadium. San Jose won.
the oval park in stanford university - stanford california stock pictures, royalty-free photos & images
Cyclist rides by a map of the Stanford University campus on March 12, 2019 in Stanford, California. More than 40 people, including actresses Lori...
The Stanford logo is displayed on a track on the Stanford University campus on March 12, 2019 in Stanford, California. More than 40 people, including...
General view of the Stanford University campus including Hoover Tower before a NCAA Pac-12 football game between the Stanford Cardinal and the...
stanford university, hoover tower, palo alto and the south bay - stanford california stock pictures, royalty-free photos & images
silicon valley 3d landscape view east-west natural color - stanford california stock pictures, royalty-free photos & images
The Lu Ka Shing Center for Learning and Knowledge building at School of Medicine at Stanford University in Palo Alto, California, USA.
Stanford Hospital, Stanford University, California.
Exterior view of Stanford University on September 9, 1990 in Palo Alto, California.
Stanford Cardinal quarterback Davis Mills looks to make a pass during a game between Northwestern and Stanford Football at Stanford Stadium on August...
Chairs sit empty outside the Dean of Students Office during a quiet morning at Stanford University on March 9, 2020 in Stanford, California. Stanford...
Study space remains closed due to Coronavirus fears at Stanford University on March 9, 2020 in Stanford, California. Stanford University announced...
Quarterback John Elway of Stanford University throws a pass during the 85th Big Game against Cal played on November 20, 1982 at Memorial Stadium in...
Declassified reconnaissance satellite view, taken by the Central Intelligence Agency's Keyhole spy satellite of Stanford University and a portion of...
The California Golden Bears and the Stanford Cardinal face off at the line of scrimmage during the 122nd Big Game on November 23, 2019 at Stanford...
Jaylinn Hawkins of the California Golden Bears celebrates with the Cal fans after they beat the Stanford Cardinal at Stanford Stadium on November 23,...
Colt Doughty of the California Golden Bears celebrates with the Cal fans after they beat the Stanford Cardinal at Stanford Stadium on November 23,...
Ed McCaffrey of the Stanford Cardinal catches a touchdown pass with 12 seconds left in the 93rd Big Game between the California Golden Bears and...
General view of the University of California Berkeley campus including Sather Tower, also known as The Campanile, as seen from Memorial Stadium...
California Golden Bears linebacker Evan Weaver celebrates in the final moments of the college football game between the California Golden Bears and...
colorful palo alto city art map - stanford california stock illustrations
Leonard Williams of the USC Trojans walks down to the tunnel with his teammates to warm up for their game against the Stanford Cardinal at Stanford...
General view of the campus of Stanford University including Hoover Tower and buildings of the Main Quadrangle before an NCAA Pac-12 college football...
People walk by Hoover Tower on the Stanford University campus on March 12, 2019 in Stanford, California. More than 40 people, including actresses...
silicon valley 3d landscape view south-north natural color - stanford california stock pictures, royalty-free photos & images
People play soccer near Hoover Tower on the Stanford University campus on March 12, 2019 in Stanford, California. More than 40 people, including...
hallway in stanford university - stanford california stock pictures, royalty-free photos & images
General view of the Stanford University campus including Hoover Tower as seen from Stanford Stadium prior to an NCAA college football game between...
Graduating Stanford University students attend the 128th Stanford University commencement ceremony on June 16, 2019 in Stanford, California.
Person walks towards the main quad during a quiet morning at Stanford University on March 9, 2020 in Stanford, California. Stanford University...
Stanford Cardinal head coach David Shaw leads his team out onto the field at the start of the game between the California Golden Bears and the...
Reading room is seen at the Cecil H. Green Library on the Stanford University Campus December 17, 2004 in Stanford, California. Google, the internet...
International students Yaqing "Victoria" Yang and Ende Shen of China study together at a sidewalk table in the Silicon Valley city of Palo Alto on...
empty walkway with columns at stanford university - stanford california stock pictures, royalty-free photos & images
Graduating Stanford University students turn around to thank their parents during the 125th Stanford University commencement ceremony on June 12,...
memorial church framed by arch, stanford university, san francisco, california, united states of america, north america - stanford california stock pictures, royalty-free photos & images
People pass by the Hoover Tower on the Stanford University campus December 11, 2002 in Stanford, California. Stanford announced plans December 10,...
Sorry, your search returned zero results for "stanford california"


text:
Clarifying Medical Bankruptcy
Medical bankruptcy is a much-debated topic, with most questions focused on exactly how many people file for it and how often it occurs. In 2005, Elizabeth Warren and her colleagues found medical costs led to over 40% of bankruptcies in the United States. This was followed by an update in 2009, pushing the proportion of bankruptcies due to medical expenses to 62%.
The Consumer Financial Protection Bureau's 2014 report conflicts with this, citing that less than 1% of US adults file for bankruptcy even though 20% of the population has great medical debt. A group of economists recently reexamined this issue, concerned that the discrepancies in statistics were causing a misunderstanding of the problem. They studied a group of patients at a California hospital and looked at how hospital visits related to bankruptcy timing.
The image above shows an increase in people filing for bankruptcy after hospitalization, particularly between one and four years after admission. The researchers suggest that paying for medical bills out of pocket, and losing income because of missed work are key reasons people file for personal bankruptcy. The graph also shows, however, that only 4% of the bankruptcies were related to hospitalization, an association of much smaller magnitude than previously understood.
Warren and colleagues critiqued the economists' research, stating that focusing only on hospitalization does not account for other medical experiences and expenses like spending time and money in emergency departments, and paying for chronic illness treatments. The economists' subsequent response argued that estimating a causal relationship requires focusing on an isolated factor, like hospitalization.
Databyte via Carlos Dobkin, Amy Finkelstein, Raymond Kluender, and Matthew J. Notowidigdo, Myth and Measurement — The Case of Medical Bankruptcies. New England Journal of Medicine.
Older Moms
It Works: Innovative Medical Technology's Impact on Global Health


text:
TechTalks With Tom Smith: Issues in Migrating to Microservices
People, determining service size, identifying dependencies, monitoring, and data.
Tom Smith
CORE ·
Sep. 17, 19 · Analysis
We have issues (with migrating to microservices).
To understand the current state of migrating legacy apps to microservices, we spoke to IT executives from 18 different companies. We asked, "What are the most common issues you see migrating legacy apps to microservices?" Here's what we learned:
You may also like: Migrating to Microservices? Here's How to Have Reliable APIs From Day One
You are going from an army of sysadmins to spinning up and managing infrastructure not directly under your control. There's an evolution of the sysadmin role. Get data in the right format in the right places. This is why infrastructure as code is gaining popularity. Make it declarative in nature to make it easier.
People either try to rewrite and fail miserably or just do greenfield with no plan for integration. The new team doing microservices ends up extending the monolithic application because management gives up on the integration and ends up telling everyone to keep working on the monolithic app. Twitter and Lyft were successful because they made the transformation gradually.
During the analysis phase, you learn a lot of legacy apps were designed and assembled by people who have left the organization. The way applications are stitched together is poorly documented and people have trouble understanding the anatomy of their legacy apps. Another challenge in understanding microservices is there's a lot of hype. People attempt to just convert legacy apps without understanding the need to rethink how an application is structured and designed. They expect an easy transition without understanding the principles. There's a huge learning curve.
Lack of pragmatism about the problems you are trying to solve. Lack of documentation. Microservices are all about trust. What's available in the enterprise. Poor documentation results in no trust. You are unable to leverage each other's work. Documentation becomes a trusted authority within the enterprise. We help developers keep documentation up to date. Use machine learning (ML) to learn and update documentation by listening to traffic and creating the documentation. Documentation is not seen as valuable. Documentation is not a "nice to have," it's part of the product — what it does, how to consume, and how to use it. If systems are not performant and fast, slow is the new "down." Outstanding application performance is key to great user experience.
Service Size
Identify the service size. It should be as small as needed but no smaller. You have all the advantages of each team having a tech stack, but you also have complexity from a traffic standpoint across the datacenter. Ensure you have a handle on traffic, which there is a lot, and monitor performance, reliability, caching, and routing to ensure high availability.
People, technology, and infrastructure. Microservices is driving the conversation around DevOps and CI/CD. Understanding how much to break off has to match the business problem to solve and the structure of the organization. Size the service to meet the need.
The most common issue we see when migrating legacy apps to microservices is the maintenance challenges that result from the initial plan to minimize the architectural change. For example, if a legacy app consists of five modules, the natural direction for the new architecture is to build five microservices, which is often not the correct design. Following a service-oriented architecture (SOA) also creates challenges, as SOA is ideal when your applications need to communicate with all other applications, versus a microservices architecture where each microservice only needs to serve data to a specific set of consumers. By continuing a monolithic application mindset, you don't truly take advantage of microservices and often just create more overhead as a result of the inefficient design.
1) Dealing with complex middleware (ESB/SOA) that no longer is required but is part of the current implementation. 2) Understanding the legacy application and deciding which use cases are necessary and which are nice to have.3) Understanding the business logic that goes with the legacy system (regulatory or security concerns, etc.).4) Breaking down the monolithic application into small, distinct pieces for a real microservices architecture.
It's not obvious where to draw the lines separating between potentially independent domains in existing software. Often using a shared model across different areas of the application makes for very tightly coupled design. This can even be dramatically exacerbated when using an ORM system, where the model is sometimes correlated with the database schema. Implicit transactional boundaries, provided by some popular frameworks, often contribute to an entanglement that's very difficult to clear up.
The flow of data in and out of the system is also a major factor in being able to break down legacy apps into independent microservices. Each microservice should be able to store and retrieve its data independently of the rest of the system. For that to take place, the sources of data for each microservice need to be clearly delineated. That's not an easy thing to do. Propagating and consuming events is often the go-to solution for these issues but it's not trivial to adopt.
Tenacity, you have to see it through to completion when things get scary. Consider the move to microservices as experiments and learning exercises. Someone in middle management and IT pull the ripcord. Monitoring becomes a huge issue because it reduces worry. So companies may not have any monitoring at all. If you can't provide replacement data and signals from microservices, ops are going to resist. Make sure you provide robust instrumentation inside the application.
One common issue is that migrating to microservices is a bit of a cultural shift, as the legacy applications may have been around for many years and some IT teams can be reluctant to change. Ultimately the shift needs to be made as demand for fast, intuitive, and elegant applications are not slowing down. Monitoring the application is even more critical as one microservice can cause an issue somewhere else. When you break apart a monolithic application into many microservices you can quickly see how this is a concern, so putting a monitoring solution that covers all aspects of on-prem and cloud is critical to helping IT Operations reduce the time of root cause analysis and understanding all the dependencies.
People think the new microservices will behave the same way as the legacy app. Multiple services are interconnected. Unless your app and workload are consistent you can have misaligned expectations. Scaling databases requires storing data for microservices in a single node. Think through what the database recovery will be.
Figure how to communicate between services to ensure they synch and deploy automatically, have the right code at the right time. There is a lot of complexity required to manage a suite of services. Management overhead is the biggest issue that comes from moving from one to multiple services and how to communicate between services that do not share memory.
Scalability, fault tolerance, and geographic distributions. Day two operations are quite different with microservices than with a traditional application.
It's important to understand the difference between north-south traffic (into and out of the application environment) and east-west traffic (between services within an application) when it comes to security, identity, routing, and service discovery. Last-mile policies enforced by service mesh and other local infrastructure tools are not a substitute for edge-based technologies that manage and secure the application when it's exposed to broader audiences.
Microservices can improve agility, but they aren't for every organization or application. When starting with microservices, it's important to remember that they require significant development and delivery skills, including implementing proper security measures, building a mature DevOps environment, and enforcing a high degree of standardization and automation using methods such as CI/CD and technology such as containers and Kubernetes for container orchestration.
Don't migrate everything. It may not be worthwhile to refactor very old applications that are built with old languages and databases. These applications may be worth rebuilding from scratch rather than migrating them.
Another challenge is migrating more complex legacy distributed applications that run in an on-prem Data Center-centric infrastructure to a distributed application architecture using cloud-centric technologies deploying K8s applications seamlessly across multi-cluster environments. Moving to the cloud offers many advantages, but there are significant startup costs and learning curves to navigate in order to successfully transform from legacy distributed apps to modern distributed cloud-based microservices apps.
1) In many cases, microservices migration requires architecture and code changes which can lead to long development cycles. 2) Microservice orchestration (deployment, upgrades, rollbacks) require more effort compared to monolithic architecture.3) Operations, diagnostics, debugging require new tooling since a single computation or request can touch multiple isolated microservices. It is harder to follow the request through the infrastructure, compared to the monolithic application. It is important to have proper auditing and tools to get visibility into the computation.
The most common issue is applying microservices architecture to every application, just because it is the "in-thing" or because of perceived benefits. Careful evaluation is necessary since the development, operation, and maintenance of a complex microservices-based application can become an expensive white elephant if not designed properly. The second most common issue is how to migrate — do we rewrite the whole app, or do we do it piecemeal? Rewriting from scratch has many issues — the "why" of some of the features may be difficult to reconstruct, the schedule for the new app may be uncertain. But the biggest challenge is that Business may not fund the rewrite — after all, the old one is working fine for now!
Here's who shared their insights:
Gregg Ostrowski, Regional CTO, AppDynamics
Jaime Ryan, Head of Strategy, Layer7 Security and Integration, Broadcom Enterprise Software
Sanjay Challa, Director of Product Management, Datical
Dale Kim, Senior Director of Product Marketing, Hazelcast
Marco Palladino, CTO, Kong
Karthik Krishnaswamy, Director of Product Marketing, F5
Joe Leslie, Senior Product Manager, NuoDB
Zeev Avidan, Chief Product Officer, OpenLegacy
Matt Yonkovit, Chief Experience Officer, Percona
Bich Le, Chief Architect, Platform9
Sridhar Jayaraman, VP of Engineering, Qentelli
Anurag Goel, CEO, Render
Patrick Hubbard, Technical Product Marketing Director, SolarWinds
Idit Levine, Founder and CEO, Solo.io
Markku Rossi, CTO, SSH.com
Nick Piette, Director of Product Marketing API Services, Talend
Ophir Radnitz, Software Architect, Tufin
Karthik Ranganathan, Co-founder, and CTO
The Future of Microservices Migration
Microservices Migration Use Cases
microservice application app
Distributed Stateful Edge Platforms
Project Hygiene
How To Validate Three Common Document Types in Python
Top 5 Node.js REST API Frameworks


text:
An Evening with Kathryn Claire – Saturday April 14, 2018 at 8:00pm
April 16, 2018 Prior ShowsAmber
Featuring Allen Hunter (bass) Don Henson (piano/percussion) Sid Dilson (violin).
Kathryn Claire has spent years cultivating her own style and approach to music as a violinist, guitar player, singer, and songwriter. Strong fundamentals from her classical and traditional music background combined with improvisation has made her a favorite at venues, festivals and institutions around the world. She has toured and performed extensively in the US, Japan, India, Holland, Belgium and France.
In her latest album "Bones Will Last," musician and composer Kathryn Claire has created a unique collection of songs and instrumental compositions. With her violin and voice at the forefront, Kathryn is supported by Zak Borden on mandolin, Allen Hunter on upright bass, and Don Henson on piano.
"Bones Will Last" is a hopeful and heartbreaking album, exploring deeply both personal and universal themes of loss, love and transformation. Kathryn Claire skillfully weaves together stories and melodies rooted in her classical and traditional musical background. Her honest and poetic writing and her unique voice move seamlessly across genres creating an aesthetic which is original and diverse. The ten tracks on "Bones Will Last" draw from her extensive international travel over the past 10 years, and synthesize her personal and musical history.
"Claire's deep vocals combine with exquisite layered orchestrations. These dark, provocative, thoughtful songs engage the listener and elicit deep emotions."
-Amy Steele, ENTERTAINMENT REALM
"They bring to the music a vital and joyous creativity that excites even the hardest of hearts." -John Doyle, founding member of Solas.
"The instrumentals play just as profoundly, perhaps more effectively, as if stepping lightly around the graves of the forgotten and the missed."
-Carol Banks Weber, MEDIUM
"Claire's song's and instrumental arrangements, blessed with a fine back-up band, flow into one another in a highly emotional way, the instrumentals containing a dark beauty about them, while the songs burst into melodic gusto, the two continually born of one another."
-Dinah Urell, HIPFISH MONTHLY
www.KathrynClaireMusic.com
← Molly's Revenge – Saturday March 10, 2018 at 8:00pm	The Quitters – Saturday May 12, 2018 at 8:00pm →