In previous articles I showed you how to develop custom PowerShell cmdlets using Visual Studio. In this article we will cover how one can go about creating custom function using native PowerShell scripts. The method we will create will accept piping parameters to it in order to fully leverage the power of PowerShell. To demonstrate this, we will go and create a new PowerShell function name Get-SPListItemCount that will receive and SPList object as an input parameter, and will output a custom PowerShelll object containing two parameters: the list title, and the number of items contained within it.
From the code above, we start off by declaring function Get-SPListItemCount. Then to start off the function declaration, we specify what parameters our method will be accepting, in our case a single parameter, named $list which represents the received SPList object for which we wish to obtain the item count. Using the Parameter, we specify three very important settings. First, that the parameter is mandatory, meaning we require the user the pass in at least one parameter, second that the parameter can be received by the pipeline (using the PowerShell '|' operator), and third that the parameter received will be assigned to the $list variable within the function.
Then using the [PSCustomObject] operator, we ensure that our function returns a custom PowerShell object that will contain two properties: the Title of the list received as a parameter, and the ItemCount property of that same list which represents the total number of SPList item contained within the list.


Before the Persons Case of 1929, women weren't considered Persons.
Officially, they did not belong in the Senate. Women belonged in the kitchen, in makeup, and with the children. That all changed when the Famous 5 bravely demanded that women be considered Persons, making them eligible for all positions of government. Now women legally belong in any role their male counterparts do, but in reality are often underrepresented.
If women belong anywhere, why aren't they everywhere? Raise your voice to raise the numbers. Let's show that #WomenBelong.
Connie DeSousa received her Le Cordon Bleu Paris Certification at SAIT in Calgary then got experience from kitchens in Germany, New York, and California before returning to Calgary to open CHARCUT, and then charbar, with co-owner and co-chef John Jackson. For the first few years, when customers asked to see the chef, and she came to their table, they would often say "No, sorry, I asked to see the chef." Now, people ask for the Executive Chef by name.
Kate Hurley has been an infantry reservist, or foot soldier, with the Canadian Armed Forces for four and a half years. Many times throughout her training Kate was one of very few women, but she faced the same obstacles as everyone else, and had to overcome them the same way everyone else did: with mental perseverance, resilience and hard work.
The first time the Calgary Fire Department held a recruitment campaign targeting women – who like to be physically challenged, have a fearless attitude, and work well as a team – it caught the eye of international rugby player Katrina Holmquist. Her training began shortly after the birth of her son, making the physical elements more challenging than anticipated, and filling her with self-doubt. When her first call was to a car accident where a young mother lost her child, she feared being a new mom made her too emotionally soft for the job. However, after six years sharing conversations with other firefighters, she has learned that her struggles are not unique to women, they are part of being human.
A young girl once told Chandra Crawford she didn't like being a girl, because it meant she didn't get to do fun things like skateboarding and had to worry about her appearance all the time instead. The Olympic Gold Medalist in cross-country skiing was inspired to pursue her passion for sport by her feminist mother, Louise, and 4-time Olympian ski racer Sara Renner, so she strives to pay it forward and inspire other young girls to find health and happiness through sport.
Throughout her education and career, Sharron Spicer has had both male and female mentors who modelled compassion, showed dedication and propelled her to excel in her field. She is pleased that, thanks to the women before her and other women like her, the current generation can consider the field of medicine without regard for gender.
Carmen Brauer is an orthopedic surgeon who practices at the Alberta Children's Hospital. She always puts herself in her patients' shoes to determine the best course of treatment for their needs and lifestyle. When it comes to hospital-firsts, Carmen steps up to the challenge, like in 2013 when she performed the first bone lengthening in an upper extremity in the Alberta Children's Hospital's history.
Heather Gallant splits her time between the office and the field, managing the environmental and regulatory division of an oil and gas engineering firm. Her professional journey included shift work at a large oil sands development, where she lived in a 5,000-man camp for 21 days at a time, but she is often assumed not to have this hands-on work experience because of her gender. Once she conveys she has walked the walk, she is treated with respect, despite often being the only woman in meetings.
Sandra Jansen is the voice for Calgary - North West in provincial matters and the opposition critic in the areas of education, human services and women's issues. As the former Associate Minister of Family and Community Safety, she released the province's first domestic violence framework. As a single mom, she understands the importance of a strong social safety net.
Madam Justice Patricia Rowbotham has practiced law at various firms, taught at the University of Calgary, served on the Court of Queen's Bench of Alberta, and has now been appointed to the Court of Appeal of Alberta, the Northwest Territories and Nunavut – the highest court in the province. Despite great progress in the representation of women in law, Patricia still sees room for improvement and takes her role as a mentor to young women seriously. One of her key pieces of advice to young women is that "confidence matters as much as competence".
When Dianne Wilkins took a job with Critical Mass at their office in Sweden, the new overseas operation needed a leader, and she quickly rose to the top – despite being the youngest person in most meeting rooms and probably the only female. Soon she became Chief Executive Officer, a position she has now held for 10.5 years, growing the agency from 25 people in Canada to 850 employees around the world. Di advises people to speak up for what they want and remember who they are on the push to the top.
As the Technology Lead for an application development team at Critical Mass, it is Babita's turn to mentor and motivate others. Her days are a balance of hands-on development and overseeing the work done by the rest of her team. To her, "being a women in the tech industry is awesome".
The most important of Rachel-Jennifer Joson's many responsibilities is to ensure her children are given quality time every day and are constantly reminded that they are loved and full of potential. She is proud to be raising the future's leaders.
Since 2005, Alida Visbach has led living history museum Heritage Park through its largest expansion in history. Not only did she double the physical size of the park, she enhanced the education and public programs to attract a wider demographic – including the construction of the Famous 5 Centre of Canadian Women to shine the spotlight on women in Canadian history.


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Home ›Our Books›Parenting›Global Mom
Global Mom, A Memoir
Eight Countries, Sixteen Addresses, Five Languages, One Family
Melissa Bradford
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After more than twenty years living internationally—sixteen addresses, eight countries and five different languages—writer Melissa Bradford shares a fantastic journey of motherhood that will inspire any family.
Follow this family of six on their passage—extraordinary, hilarious and heartbreakingly poignant—from Bright Lights (of New York City) to the Northern Lights (of Norway) to the City of Light (Paris) to the speed-of-light of the Autobahn (in Munich). Continue deep into the tropics of Southeast Asia (Singapore) and end your voyage in the heights of the Swiss Alps (Geneva).
As varied as the topography—the craggy fjords, the meandering Seine, the black forests, the muggy tropics, the soaring Alps—this multicultural tale traverses everything from giving birth in a château in Versailles to living on an island in a fjord. From singing jazz on national Norwegian T.V. to judging an Indonesian beauty contest. From navigating the labyrinth of French bureaucracy and the traffic patterns of Singapore to sitting around a big pine table where the whole family learns languages, cultures, cuisines—where they, in short, learn to love this complex and diverse world and, most importantly, each other.
Praise for Global Mom, A Memoir
"This could have been a memoir about loss, and a mother's grief. It would have been natural and understandable, given that her son, Parker Bradford, died suddenly and unexpectedly at the age of eighteen. Any parent brave enough to try to imagine that loss would have forgiven Melissa Dalton Bradford for being unable to write from any other point of view than that of sorrow. Moreover, I have no doubt that book would also have been worth reading, since Melissa Dalton-Bradford writes very well. Instead, here is a rich, frank and funny book in which the essentials of family and friendship and community are combined with interesting travelogue and the best kind of spiritual writing. In short, this is a book about love." —Kate Braestrup, New York Times best-selling author of Here If You Need Me
"After twenty years and eight different international relocations for her husband's career, Melissa Dalton-Bradford has much to offer on how ordinary family moments can create an extraordinary family journey when you mix countries and cultures. Global Mom: A Memoir is a brilliant hero's journey highlighting the challenges and triumphs of motherhood under unique cross-cultural circumstances. With honesty, sensitivity, and humor, Dalton-Bradford is a role model for all parents who will be relocating with children, especially those who will relocate for their spouse's career." —Paula Caligiuri, P.h.D., author Cultural Agility: Building a Pipeline of Successful Global Professionals
"Global Mom provides an honest and poignant look at the unique challenges of raising a family across multiple cultures. It's a journey worth visiting for readers." —Bicultural Mama
"The humor is self-deprecating; the pain—beyond compare. I found myself laughing out loud. . . and sobbing out loud, as well." —The Association for Mormon Letters
". . . a stunning picture of life . . ." —The Deseret News
". . . a must read . . . a powerful story . . . extraordinary." —Chuck Lit Central
"After reading Melissa Dalton Bradford's fascinating memoir of her adventures with her family I am left with many emotions—admiration, amazement, and, as a mom who has done her own fair share of moving her family around, deep empathy. This is one brave woman!" —Sharon Galligar Chance
Check out Melissa Bradford's profile!
Melissa Dalton-Bradford is a writer, independent scholar, world citizen, and mother. She holds a BA in German and an MA in Comparative Literature, both from Brigham Young University. She speaks, reads...
Global Mom Reviews

redpajama_set_name: RedPajamaCommonCrawl


Cathy Yang is currently the head of the commercial company of Shanghai Tower. Before joining Shanghai Tower, she had been in charge of TAIPEI 101's operation for 15 years. She also took TAIPEI 101 on the journey to become the tallest LEED EB Platinum green building in 2011 and started the re-certification process in 2014. She also initiated the issuance of annual Corporate Sustainability Report for TAIPEI 101. In addition to the regular operation of a commercial building, every year she lead the team to launch several annual events that contributed in the promotion of the city of Taipei, including the famous New Year's Eve countdown fireworks display.
Before TAIPEI 101, she worked for an international property consulting firm in Taipei, Tianjin and Beijing for 8 years where she had extensive experience in various aspects of real estate services and had set up the Beijing operation for the firm. Cathy Yang has a bachelor degree in Economics from National Taiwan University in Taipei and a Master degree in International Affairs from Columbia University in New York.
Cathy has been involved with CTBUH since TAIPEI 101's completion as the world's tallest building at the end of 2004. She spoke at several CTBUH conferences sharing her experiences on leasing and managing a supertall building and on the greening efforts of the former tallest building. She was the CTBUH country representative and was on the board of Trustees from 2013 to 2015.
CTBUH has named its 2016 Fellows and two Lifetime Achievement Award recipients: Dr. Cheong Koon Hean of the Singapore HDB, and Ron Klemencic of MKA.
The CTBUH has confirmed the next generation of industry leaders to join its Board of Trustees: Cathy Yang, Taipei Financial Center Corp., Craig Gibbons, Arup and David Malott, KPF.


Why did I become a Hindu?
Why did I become a Hindu? Well, I can´t answer you this question with only one answer. I was born in a Catholic family and studied many religions and believes and even made part of some different belief systems before I became a Hindu. While I was getting familiar with all those different creeds, I realized empiricism ( that which you can know by verifying by yourself if it's true or not and not count only on faith) was very important at least for me, to have a more profound trust in religion or a spiritual system. Before I got into Hinduism, I had some experiences with Judaism when younger, but later on, when I was mature spirituality, I became interested in a dharmic religion: Buddhism. To be more specific, in Theravada Buddhism which is predominant in Southeast Asia like Thailand, Myanmar, and Sri Lanka. The most important teachings I have learned was about meditation and how the mind works. I went to Thailand and spent some weeks in a monastery, and after that, my meditation significantly improved.
After some years I started reading about Hinduism, but since I was a teenager, I enjoyed reading about Eastern culture, including Indian. This theme always attracted me. I realized Buddhism was a part of Sanatana Dharma and Hinduism would provide me the "whole picture." After watching some videos of a guru called Rohit Arya, I understood the importance of making part of a "parampara" or spiritual lineage. I always felt a connection to Sri Ramakrishna, so I decided to be part of his "parampara." I started frequenting the temple in my city, and after some time I´ve got the "mantra Diksha." Now I will tell about the main reasons why I became, and still, I´m a Hindu: The faith in Hinduism but more specifically in Yoga,( all kinds of Yoga like Bakhti, Jnana, etc.) is something which is based on practicality or empiricism. And not in the "blind faith" of the "Abrahamic" religions. After the first months of "sadhana," I felt already a big difference, the presence of shakti acting in my life. This is not common. I believe it was possible mainly because of my past practice of Buddhist meditation during some years and also the meditation method that Ramana Maharshi taught and also Nisidargatta Maharaj. Those two gurus are my favorite gurus of the 20th Century. Another reason for this choice is my belief that Hinduism is the spiritual path which is closest to a primordial traditional that was lost a long time ago. Hinduism is also a nondogmatic religion, the opposite of what "Abrahmanic" religions are.
All this reason I presented for me, are strong reasons to adopt Sanatana dharma as my path of life and in my opinion, Hindus who consider themselves secular should "wake up" and discover the real "treasures" that exists in Sanatana Dharma.
Ramanuja Acharya (1017-1137) was the most significant teacher on the concept of "Visista Advaita" or "qualified monism." In this school of Vedanta, he teaches that everything is Brahma although there are distinct existences between everything existing and God. Edmund Husserl (1859-1938) was a German philosopher, mathematician, and the creator of a philosophical school called Phenomenology which until now, is not fully understood by the mainstream currents of psychology and neuroscience in our present time. Ramanuja was one of the most important acharyas in the last a thousand years and obviously, an extremely spiritual person, born in Tamil Nadu. Edmund Husserl despite being a materialistic ( even though he was born in a Jewish family and converted to Protestantism as an adult) had a very similar approach to Ramanuja's point of view about our cognition about the reality. In the book "The theology of Ramanuja," the author C.J Bartley states Ramanuja disagree with a grammarian of Sanskrit called Barthrihari who lived in the 5th Century C.E concerning the nature of the written language. Ramanuja believed there is a separation between language and our cognition while Barthrihari believed language and consciousness were inseparable. The Tamilian scholar also taught that the real meaning of the language was in words and Barthrihari stated that sentences (a group of words) were the representations of reality in the language. Edmund Husserl agreed with Ramanuja both about the distinction between the language and our cognition and about the function of the words in the language. (Although the last one, in an indirect way) For this German philosopher, in the human psyche, each word represented the essence of that thing which the word was representing although there is a separation between them. For Husserl, the relation between the object thought, and the act of "thinking" was called "intentionality," and for him, the essence of logic was in the "world of essences" which was beyond the human psyche and language. This idea is very similar to the opinion of Ramanuja concerning language and cognition of the reality. How is it possible that two persons that lived in an 800 years span gap in entirely different cultures and a completely different social environment had same ideas in such peculiar points concerning reality?
The German philosopher also was a voracious critic of the modern philosophy and modern science that started arising after the 17th Century and reached a "materialistic peak" at the beginning of the 20th Century. The modern philosophy which was born in the last 300 years also gave birth to the modern science. To the German philosopher, science today is stuck in a very abstract and materialist point of view, and because of that, it can´t develop any further if the Western thought continues in this pattern. As everybody knows, modern philosophy greatly limits the spiritual development of the society nowadays especially because of the separation which it imposes between the mind, an internal reality and an external. However, even in the modern science, some theories raised which contradicted this separation which started with the French philosopher Descartes in the 17thCentury. The Nobel prize winner Wolfgang Pauli, a great quantum physics scientist, in an exchange of letters with the psychologist Carl Jung, suggested mind and matter were the "same sides of the same coin." Another great quantum physics scientist, David Bohm, (whom Einstein stated he understood quantum physics thanks to Dr. Bohm) created a theory called "Implicate order." This theory states that fundamental forces control the universe, forces which permeate the whole space, the last one is not empty according to do Dr. Bohm, but is filled with an invisible "sea of cosmic energy" that is constantly acting upon the visible world. Rupert Sheldrake, a biologist, created a very similar theory which he called "morphogenetic field." All these scientific hypotheses corroborate with the theory created by Husserl and why not, also support the point of view of Ramanuja Acharya about reality.
If we consider those scientific hypotheses, the theory of Husserl and the "Visista Advaita" or "Qualified monism" then we can answer that question which closed the first paragraph of this essay. Some invisible "forces" control everything that happens in our perceivable dimension, and by understanding this, we see that it is not strange that two persons living in an 800 years time gap, in completely different circumstances, come to the same conclusion about such a complex theme. However, the mainstream science that was born in modern philosophy has a very arrogance approach towards these ideas. Despite this skeptical challenge, the tendency is through future, in decades, scientists are going to accept better these new current of thoughts. The reason for this is because the Cartesian thought that dominates science is almost hitting a "dead end," mainly because of the new challenges quantum physics brought. And when this happens, society for sure will be more open to Sanatana Dharma.
The role of Hanuman and Narasimha nowadays: A call for us, Hindus to wake up!
We see images of Hanuman everywhere in India nowadays. This deity was one the greatest warrior of all times, and he is the main hero in Mahabharata, despite the massive importance of avatar Rama of course.The Hindus living in India know the reason behind it: the unfair way which Hindus in the country has been treated in the last decades since independence. Finally, people are reacting to it. Hanuman is considered to be the avatar of Shiva and among the Vaishnavas, the avatar of Vishnu which embodies better this "Kshatrya trait " is Narasimha, the "lion-man" who came to the earth to restore the dharma and fight evil.Indian Hindus also should remember this last one try to grasp the deepest meaning of his coming to this planet. We are living a time in history which the main qualities of a "Kshatriya" as courage, witness and strength are essential for us, Hindus to protect Sanatana dharma against "asuric" forces. The religious Hindus (not "secular Hindus") in India know what I am saying here.
However, the quality "strength." in this case we are living nowadays is the mental strength, an intellectual fierceness which the fathers of Indian independence like Sri Aurobindo and Bal Gangadhar Tilak had to struggle not only for the independence of the country. They knew that India´s independence was only the beginning, especially Sri Aurobindo because he predicted India´s future as the "Jagadguru" of the world. Unfortunately, many Hindu Indians are not aware of that, and they must "wake up" as soon as possible, not only for the good of India but for well being of the world. That´s because Sanatana Dharma which goes beyond the Hindu religion, it is the way which connects us to the cosmos and brings a balance to our existence. And this balance is what is going to save us from destruction as I mentioned in one of my previous essays on this website.
I feel that Hanuman is helping me with my mission as he is also assisting many people who are struggling to defend Sanatana dharma in this critical time we are living. One of his roles is to overlook the evolution of humankind.And he also gives strength and intelligence to people who sincerely defend Sanatana Dharma as he defended so heroically serving so wholeheartedly his dear Rama. About the avatar of Vishnu Narasimha, I believe is interesting to remind that lion is also considered a sacred animal in other mythologies besides the Hindu. The fierceness which he ripped open the belly of that powerful demon is the spirit in which we should engage in our struggle to defend Sanatana Dharma in all ways possible, and each one of these ways fits for each person. I especially invite people who want to protect this sacred path in an intellectual perspective to join this cause which I am bringing on.
The great Swami Vivekananda in the 19th Century was the first world-famous personality to emphasize the need for Indians raise their self-esteem, unite among themselves and raise the nation. Later on, Sri Aurobindo mentioned about the important role that India would have in the future. Among specialists in geopolitics like Nicholas Spykman, (1893-1943) mentioned the importance of India because of her especial geographical position and the great potential the country has because of it. Some financial institutions are predicting India will be the third world economy by 2050, behind only to U.S.A and China.
However, the real strength of the country is not economical or geopolitical although those are important aspects for the projection of Bharat in the world. The real source of power to India its spirituality, or to be more specific, Sanatana Dharma. At the end of the 19th Century and beginning of the 20th Century, when the movement for independence was starting to gain momentum, the people responsible for that like Bal Gangadhar Tilak and Bipin Chandra Pal understood the importance of the role of Hinduism in this political initiative. The reason for this is because they knew Sanatana Dharma was the vital force that keeps this nation alive, even when is subjugated by some foreign power like the British Empire at that time. However, when we talk specifically about the 21st Century, the main point is this one: The fusion between men and machine or the blend between the human consciousness and artificial intelligence that some are predicting will happen around 2045. This future happening is going to bring a huge shift in the way we perceive the meaning of what being human is. We are living in a nihilistic and materialistic society where true spirituality is scarce, and this is uprooting the global human consciousness from its true source, the spiritual source. To prove this statement,even materialistic historians when talking about the pre-history and the rise of a unique cognitive consciousness (which animals don't have) in the mind of the "Homo sapiens",agree on the religious rituals which they started to perform during the burials was one of the most meaningful signs of the rise of this new human conscious.
Sanatana Dharma is the only real and true spirituality which bought an order on how human must live to have a harmonious life for many thousands of years.It goes beyond: This holy path teaches us how to attain liberation or "moksha" step by step in a way which is not dogmatic.We can realize annalizing all that we mentioned here, the crucial role of Hinduism not only for India but the future of humankind because if we lose our sense of humanity, the only fate for us is going to be destruction.
Rajiv Malhotra in his book called "Being different" presents to us the dharmic concept of "Purva Paksha" which is a method of counter-argument used in the past by the ancient Indian philosophers, including the great Adi Sankara Acharya in his famous debates. "Purva Paksha" consists basically of adapting one´s view of his opponent´s perspective, trying to have the same view of the last studying very methodically his way of thinking.By knowing well how the adversary thinks it is possible to point the failures at his thought and then correct it.
I believe Hindus urgently should go back to the tradition of "Purva Paksha" and learn about the most vital points in Western philosophy and Western ideas on social organizations. Shortly,I am planning to deliver a course on Western philosophy focusing more on modern philosophy because most of those academics and journalists who attack Sanatana Dharma get their main ideas from the modern Western philosophy.It´s time for us to wake up!


He has taught a wide range of subjects from social studies, English, French, and history, to physical education and music. He believes every academic subject offers its own unique way of communicating different life lessons and values to young people. Getting students to become aware of this concept is a challenge he truly enjoys.


De Vere Venues says it has become the first venue group to support the Business Visits & Events Partnership (BVEP)'s Britain for Events campaign.
The group, which run 33 venues across the UK, joins ranks with the campaign's supporters, which include Visit England, Visit Scotland and Excel London.
BVEP chairman Michael Hirst said: "De Vere Venues is the latest in a number of high profile brands in the UK events market to support this year's campaign; their involvement will add national reach to the campaign and direct access to people who both attend and organise business events."
The Britain for Events campaign launches on 27 October. MP Nick de Bois will use the occasion to make a speech focused on how the government can better support the UK event industry.


A holiday house in Vorarlberg costs on average GBP 1,046 in the cheap travel period and GBP 2,370 in the peak season per week. These details are of course in relation to the house and not per person as well as includes the obligatory additional charges.
A winter vacation to Vorarlburg or its capital Bregenz, can be filled with skiing, winter hiking, ice skating and other winter sports. Holiday houses or holiday appartements in Vorarlburg give visitors a home base so they can take full advantage of all that the region has to offer. A vacation in holiday homes gives visitors the flexibility to explore both the charming Austrian towns and the surrounding mountains. Holiday houses in Vorarlberg are easy to book and rent.
Vorarlburg in the winter is a frozen wonderland full of outdoor activities. The main attraction is the skiing, visitors can ski mountains known for their diverse terrain and long runs. Advanced skiers can spend a day mountain touring while beginners can improve their ski skills at the ski school. Visitors can spend all day on the slopes before relaxing at their holiday rentals or finding an apres ski party.
After a long day in the mountains visitors will appreciate having all the comforts of home at their holiday rentals. If visitors want a break from skiing they can try the winter hiking, snow shoeing and ice skating around Vorarlburg, all of which are an easy day trip from Vorarlburg holiday homes. The holiday season is a particularly popular time to visit. The Austrian village lights up with an Advent Market making Vorarlburg look especially picturesque with the snow capped mountains in the background. Visitors can walk through the decorated village and then return to their holiday homes to celebrate with their friends or family in the comfort of holiday apartments..


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« WE'D ONLY BE UNPRODUCTIVE FOR HALF THE DAY, INSTEAD OF THREE QUARTERS: | Main | WE ARE ALL DESIGNIST NOW: »
THE ACCIDENTAL HAGIOGRAPHER:
Rick Perlstein: "Ronald Reagan absolved America almost in a priestly role not to have to contend with sin. The consequences are all around us today" : From climate change to foreign affairs, Reagan pushed America toward easy lies, just as reckoning seemed possible (DAVID DAYEN, 7/30/14, Salon)
So this is a book about America's loss of innocence and, simultaneously, America's striving for a return to innocence. How do you reconcile that?
Well, that's the narrative of the book, I would say. The story I'm telling is unfolding along that loss of innocence. But the baseline is this moment in 1973 when the Vietnam War ends, and that spring, Watergate breaks wide open, after basically disappearing from the political scene for a while. You have this remarkable thing, where Sam Ervin puts these hearings on television. And day after day the public hears White House officials sounding like Mafia figures. That same spring, you get the energy crisis, and you hear officials say that we're running out of energy when heretofore, nobody knew you could run out. That's a blindsiding blow to the American psyche. And then there's the oil embargo, suddenly a bunch of Arab oil sheiks decide to hold America hostage, and succeed. So the way I characterize that is that we had this idea of America as existing outside of the rules of history, as a country that can't do any wrong. Suddenly we begin to think of ourselves as just another country, not God's chosen nation. I have a quote in the preface to the book by Immanuel Kant, who defined the Enlightenment as "man's emergence from his self-incurred immaturity," basically the process of leaving childhood and becoming a grown-up. And that's what we're seeing in America in the 1970s.
This is a remarkable juncture, and you could see it in popular culture. Like "M*A*S*H," and how it takes on militarism. People were insistently following the Watergate hearings, which were enormously complex. And America is really beginning to take on big problems, thinking about what it would mean to conserve energy, to create energy independence. Then everything takes a turn, Reagan is introduced, and he says don't worry about this stuff. America is that shining city on a hill.
We haven't received our review copy, but I have been enjoying the reviews and the controversy over Friend Perlstein's reasearch and attribution methods. As you can see here, the premise of this volume is not only hilarious but inflates Ronald Reagan into a mythical hero far moreso than any of the fawning texts we on the right produce : the gnostic reality, known only to the Left, is that America is nothing special and, for one brief shining moment, in the 70s everyone was about to realize that, but Reagan, through the exercise of little more than his personal will, restores the delusion that America is more important than other states.
If Ann Coulter or Rush Limbaugh had given Reagan that much credit for reshaping the world around himself, they'd be dismissed as overenthusiastic cultists. But Reagan looms so large in the mind of the Left that Friend Perlstein can't see he's gone far beyond any Reagan fanboy of the right in his claims for the greatness (let's say we use the term in its value neutral sense) of the Gipper.
A Liturgy of Absolution (lareviewofbooks.org)
The 'Bridge' From Watergate To Reagan, Masterfully Drawn (wnyc.org)
The right's "plagiarism" scam: How low it will stoop to protect Reagan's legacy (salon.com)
Perlstein's book is catnip for Reagan buffs (stltoday.com)
How Ronald Reagan turned America into a nation of children (theweek.com)
Twenty Feet Tall! (openlettersmonthly.com)
Night in America (washingtonmonthly.com)


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Lorient 0 Troyes 0 (1-2 agg): Goalless draw sees visitors promoted to Ligue 1
May 28th 2017 5:34PM
Troyes earned promotion to Ligue 1 after a goalless draw at Lorient secured a 2-1 aggregate success in the league's promotion-relegation play-off on Sunday.
A late strike from 40-year-old midfielder Benjamin Nivet's in Thursday's opening leg had given Troyes a one-goal advantage to take to Stade du Moustoir and they held firm to book their place in Ligue 1.
Benjamin Moukandjo struck the post in a tight first half, with neither side able to test the opposition goalkeeper before the interval.
Troyes goalkeeper Mamadou Samassa made a save from Arnold Mvuemba's free-kick and Jimmy Cabot and Moukandjo missed opportunities for the increasingly desperate hosts after the break.
And the visitors - who won their last four games of the Ligue 2 season - survived a late barrage, leaving Lorient supporters to throw flares on to the pitch towards their dejected players following the final whistle.
Troyes join Strasbourg and Amiens in Ligue 1, with Jean-Louis Garcia's men bouncing back to the top tier of French football after a single season in Ligue 2.
L'ESTAC est en LIGUE 1 !!!!!!!!!!!!!!! pic.twitter.com/bg25TXCLxk
-- ESTAC Troyes (@estac_officiel) May 28, 2017
Benjamin Nivet


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LISTEN: Exclusive Premiere of Whiskey Myers's New Song, "Early Morning Shakes"
Dan Solomon
https://www.texasmonthly.com/the-daily-post/listen-exclusive-premiere-of-whiskey-myerss-new-song-early-morning-shakes/
The last time Whiskey Myers released an album, the Tyler quintet made a splash on Billboard, debuting at number 26 on the country chart. This time out, the band's preparing its latest release, Early Morning Shakes, and they've got their eye set on bigger things: The album, which is due out in early February, was produced by Dave Cobb—whose previous credits include records by both Waylon and Shooter Jennings—and it's a bluesy collection of the drinking man's music, full of thumping drums and swaggering guitars, like what you might hear from the Allman Brothers Band if they'd grown up with a serious Led Zeppelin fetish.
Those classic rock influences are especially apparent on the album's new song, which bears the same name as the record itself. "Early Morning Shakes" may not be destined to make a big impression on a country music audience that's currently obsessed with pickups, blue jeans, and moonlight, but there are some thrills within for fans of dirty rock and roll. Singer/guitarist Cody Cannon describes the song as "the coolest song we have ever done," and explains that it's "about life on the road, or at least the life that we live on the road."
If the group left Tyler for a lifestyle consisting of regret, booze, and the DT's, they're probably exhausted just looking at their forthcoming tour schedule, which kicks off a stretch of nine Texas dates tonight in Austin. But give it a listen below and see if that sounds like a fair trade-off to you.
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Texas Monthly Staffers Featured on the Podcast 'Selena: A Star Dies in Texas' By Texas Monthly
The Dixie Chicks Urge a Drama-Free Existence on Their New Single, 'Julianna Calm Down' By Dan Solomon
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'The Nowhere Inn' Is a Meta Look at St. Vincent and Carrie Brownstein's Friendship By Jason Cohen
The Texas Tunes That Helped Get Us Through 2020 By Texas Monthly
Lomelda's Hannah Read Is Just Looking for Home By Isaac Engelberg
A Texas Monthly Blue Christmas Playlist By Rose Cahalan
Texas Outlaw Country Gets a Major Exhibit at the Country Music Hall of Fame By Dan Solomon
The Best Thing in Texas: Shea Serrano Fans Are Sending a Whole Bunch of Copies of His Basketball Book to Soldiers Deployed Overseas By Dan Solomon
The Trailer for Hulu's 'The Looming Tower' Brings Lawrence Wright's Book to Terrifying Life By Dan Solomon
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5 Bottles of Celebrity Booze Worthy of Any Texan's Bar Cart By Gabrielle Nicole Pharms


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Although Thomas Lemuel Oates started Manual Woodworkers & Weavers in 1932, the story goes back further. The roots of the company can be found in Oates' entrepreneurial spirit. He and his brother used to farm the mountain areas of Bat Cave in western North Carolina. They would also help their mother find materials for her crafts. The sons began to make wooden whistles, buckets and bird-houses. They would sell their wares along with her crafts to the people from Charlotte that came through in their horse-drawn buggies on the way to the mountains. Later, Thomas worked at the Ashville Postcard Company. When the Depression hit, he lost his job, but it inspired him to go into business and sell crafts, like cornhusk dolls and woven pieces, that were produced by the local women. He had learned about the wholesale business while working at Ashville. He built a waterwheel to generate electricity at a mill, began making product and opened shop. Over the years, he expanded the company. His son, Lemuel Oates, who would next manage the company, says he worked in the business from a young age. He explains the products were made from cotton scraps left over from making socks. Half-inch circles would be looped together to form a variety of products. Lemuel Oates went to college and then settled in Richmond. In December 1973, he returned to Bat Cave and took over the company. In 2007 his son Travis and his daughter, Molly Oates Sherrill, took over the business.
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Padenghe Boats , pen and watercolour, 5x8in. (13x20cm). Switching the 'real life' dark blue for light yellow makes the sketch far more effective.
Sir John Betjeman Statue, St Pancras Station , pen and watercolour, 8x5in. (20x13cm). Don't waste time or fret over trying to match precise colours … close enough is good enough!


Philanthropist Mary Duke Biddle Trent Semans (1920-2012) was born into a family known for its philanthropy. Her great-grandfather was tobacco manufacturer Washington Duke, a benefactor of Trinity College (now Duke University) and supporter of numerous other good causes. Her grandfather Benjamin Duke was looked to by his brother James B. and his father to direct the charitable giving for the family. Born in New York City, Mrs. Semans moved to Durham at age 14 to live with her grandmother, Sarah P. Duke. Semans developed stronger ties with North Carolina and Duke University than any other family member of her generation.
Her first husband, Josiah Charles Trent, M.D., died of lymphoma at age 34. In 1953, she married Dr. James Semans, a surgeon and associate professor of urology at Duke. The couple had three children and dedicated much of their time and resources to philanthropy and the arts. Dr. Semans helped start the North Carolina School of the Arts in Winston-Salem (now the University of North Carolina School of the Arts) in the 1960s, and chaired the school's Board of Trustees for its first 17 years. Mary Semans established the school's International Music Program in 1967. She and Dr. Semans regularly travelled across the world to support performances by School of the Arts students.
Semans' connections to Duke University were deep and varied, ranging from art history student in the 1930s to serving on the Board of Trustees from 1961-1981. Semans also supported the university and Duke Medicine through the Mary Duke Biddle Foundation (begun by and named after her mother), the Josiah Charles Trent Memorial Foundation, the Josiah Charles Trent Collection of the History of Medicine, and the Mary Duke Biddle Scholarship.
She spent decades as a trustee, vice chair, and chair of the Charlotte, North Carolina-based Duke Endowment. This private foundation was founded by her great uncle James B. Duke when he provided the endowment that transformed Trinity College into Duke University. Along with its support for Duke University, the Endowment benefits higher education, health care, children's welfare, and spiritual life in North and South Carolina.
Semans' love for Duke University was matched by her commitment to her adopted hometown of Durham. In 1951 she was one of the first two women elected to the city council, along with Kathrine Everett. From 1953 to 1955 she served as Durham's mayor pro tempore. She was a trustee of Lincoln Community Hospital from 1948 to 1976, a facility the Duke family started in 1901 to serve the needs of black patients in Durham.
My feeling is that we are all here for each other. I take very seriously this business of treating your neighbor as yourself, trying to be your brother's keeper. They're solid maxims for life. You've got to be interested in what besets other people, what their needs are.
Many have said that when they met Mary Duke Biddle Trent Semans, they felt an immediate connection, as though they knew her. It was obvious that throughout her life, she felt that same connection to Durham. She knew our community, and had an undying devotion to it, to the benefit of everyone who calls our great city home. We are grateful for her leadership over the years on many civic and academic boards, and for her contributions to health care, to civil rights and to the arts. … Truly, Mrs. Semans represented the heart, the goodness, of Durham.
She received numerous awards, including the University Medal for Distinguished Meritorious Service, Duke's highest honor; the National Brotherhood Award presented by the National Conference of Christians and Jews; the University Award from the University of North Carolina; and the John Tyler Caldwell Award for the Humanities, awarded by the North Carolina Humanities Council. She received numerous honorary degrees from universities and colleges and in 2009 was inducted into the North Carolina Women's Hall of Fame. She died January 25, 2012.


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Hugh Masekela & Wynton Marsalis: How Music Became an Instrument for Change in Mandela's Fight for Freedom
Hugh Masekela and Wynton Marsalis discuss how music became an instrument for change in Mandela's fight for freedom.
Our channel partners at Revive Music have been sharing some gems from Hugh Masekela ahead of his April 4 and April 5 retrospective at Jazz at Lincoln Center in celebration of his 75th birthday. In the clip below, Hugh and "jazz master/CBS News cultural correspondent Wynton Marsalis... sit down to explore the essential and compelling role music played during the brutal era of apartheid." As Revive writes,
When asked by Marsalis if music can change the minds and hearts of people, Masekela notes with insightful wisdom that South Africa is the "only country historically where music was a major catalyst for it's freedom." Through music, Masekela, together with Miriam Makeba, Vuyisile Mini, and countless others, responded to injustice and inequalities in a way that propelled a nation towards social change and grabbed the world's attention in unprecedented magnitude.
Masekela recalls when the late Nelson Mandela, during his time of exile in Botswana, sent Masekela a letter on his birthday. "Here is a guy who has been in jail for 20 years but he is writing to me giving me encouragement," says Masekela. He then took to the piano to write "Bring Him Back Home," the song that became the anthem for Nelson Mandala's world tour following his release from prison.
Don't miss out on Hugh Masekela's JALC shows this Friday (4/4) and Saturday (4/5) in NYC. "Each night will offer a fascinating live exploration of American jazz together with Masekela's rich heritage in Zulu folkloric styles that are masterfully infused with the mbaqanga township dance band music of his homeland." Grab 25% off tickets with the discount code REVIVE here.
Listen to Hugh Masekela's New Compilation 'Township Grooves' - OkayAfrica ›


A new species of macrocephaline ambush bug from Arizona is described.
Kormilev, Nicholas A. (1972) "A New Species of Ambush Bug from Arizona (Hemiptera: Phymatidae)," Bulletin of the Southern California Academy of Sciences: Vol. 71: Iss. 2.


On December 11th/2004 we held our 3rd annual Christmas Party at the Caledonia Train Station. The event was a big success. We want to thank all the folks that came to this event with all the food and drinks to make this night one to be remembered for a long time to come.
A special thank you goes out to Steve Geller for donating $25.00 towards the costs of the party. Another big thank you goes out to Tia for her donations of the wooden sculptures she had donated for door prizes. This really helped with the party this evening and everyone enjoyed themselves.
Down below are the pictures that were taken at the party. Wishing everyone a very Merry Christmas and a great New Year!!!!!!!
In this photo you can see the huge tree covered with lights inside the train station. I was trying to eat my dinner but ended up talking instead with Jackie and Bob. Two great newcomers that showed up.
Now here was a happy couple. Lisa and Chris that came to the party. I see the tickets on the table by Chris. He's hoping to WIN a few goodies.
It appears as though Chris and Lisa thought at first it was the cat in the hat person that came to this event, when in fact it was Alex's sister Kathy. What appears as a hat was actually one of the old signals from the tracks that gave this effect.
Alex looks like he is getting ready for going outside in the cold, and Kathy notices the camera was aimed in her direction giving a look of surprise.
Christine sitting at the back of the table trying to wave like the queen does. Keep up the great work there Christine you just might make it. Cindy over to the right of the picture was impressed at the queen's wave and started to try it for herself... Rob with the bandana on his head was wondering why all the fuss about the wave. Simon was too busy looking at one of our cards to notice the wave.


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

Millisecond pulsars (MSPs) are rapidly spinning and highly magnetized neutron stars (NSs), formed through mass and angular momentum accretion from an evolving companion star to a slowly rotating NS \citep{alpar82,stairs04,tauris11}. At the end of the accretion stages, which are commonly observed in low-mass X-ray binaries \citep[e.g.][]{tauris06,papitto13,ferraro15}, the re-accelerated NS is reactivated as a MSP in the radio bands and the companion star is expected to be an exhausted and deeply peeled star, typically a white dwarf (WD) with a He core \citep[e.g.][]{stairs04}, although deviations from this scenario exist \citep[e.g.][]{ferraro01a,ransom05,lynch12,pallanca12,pallanca13b,cadelano15a}.
Globular clusters (GCs) are the ideal factory for the formation of MSPs. In fact, the large stellar densities in the cores of GCs favor dynamical interactions, such as exchange interactions and tidal captures, which can lead to the formation of a large variety of binary systems whose evolution generates stellar exotica like blue stragglers \citep[e.g.][]{ferraro09,ferraro12,ferraro18a}, low-mass X-ray binaries \citep[e.g.][]{pooley03}, cataclysmic variables \citep[e.g.][]{paresce92,ivanova06} and MSPs as well \citep[e.g.][]{ransom05,hessels07,cadelano18}. As a consequence, the number of MSPs per unit mass in the global GC system of the Milky Way turns out to be $\sim 10^3$ times larger than in the Galactic field.

{To date, 150 MSPs are known in 28 different GCs. Among these clusters, the case of Terzan 5 and 47 Tucanae are particularly worthy of attention: the former is a stellar system known to host $\sim25\%$ of the entire MSP population in GCs \citep{ransom05,cadelano18,andersen18} and proposed to be the remnant of a pristine fragment of the Galactic bulge \citep{ferraro09,lanzoni10,massari14,ferraro16,prager17}; the latter is the second cluster in terms of MSP abundance, hosting 25 systems that allowed studies ranging from binary evolution to the cluster structure and gas content \citep[see e.g.][]{freire01,cadelano15b, riverasandoval15,ridolfi16,freire17,abbate18}}. Therefore the study of MSPs deserves special attention since it allows to study the physical properties of the host stellar system \citep[e.g.][]{freire17,prager17,abbate18} and also to probe binary  and stellar evolution under extreme conditions. This can be done, for example, through the identification of the optical counterparts, whose emission is dominated by the companion stars \citep{ferraro01a,ferraro03a,mucciarelli13,pallanca14,cadelano15b,cadelano17}. In the case of degenerate companions, like WDs or NSs, precise mass measurements of both the components of the binary can be performed directly through timing analysis if relativistic effects are observed. Such values, not only are highly valuable to study in detail the formation and evolution of these systems, but are also of extreme importance to put constraints on the equation of state of ultra-dense matter and to test general relativity \citep[e.g.][]{freire08,demorest10,antoniadis13}. If relativistic effects are not observed, mass measurements can be obtained through the optical identification of the WD companion. In fact, by comparing the observed magnitudes with appropriate WD cooling sequences, the mass of the companion star can be evaluated and such a value, combined with the mass function obtained through radio timing, provides the determination of the NS mass. { Furthermore, if the companion star is bright enough, the radial velocity curve, and thus the mass ratio,  can be determined through spectroscopic observations, together with more precise measurements of the companion mass} \citep[see e.g.][]{ferraro03b,antoniadis12,antoniadis13}.

M3 (NGC 5272) is a bright and well studied GC located at about 10 kpc from the Sun \citep[see][]{ferraro93,buonanno94,ferraro97a,ferraro97b,ferraro97c,carretta98,rood99,ferraro18b}. Its stellar population is characterized by an intermediate metallicity ($[Fe/H]=-1.5$), a very small reddening $E(B-V)=0.01$ and a large number of variable stars \citep[see][for more information about the cluster properties]{harris10}. \citet{hessels07} reported on the secure identification of 3 MSPs in this cluster plus a fourth candidate. Among these, only two MSPs, namely J1342$+$2822B and J1342$+$2822D (hereafter M3B and M3D) have been clearly detected  in a number of observations large enough to provide the astrometric and orbital properties of the binaries, although the position of M3D is still affected by a large uncertainty in both right ascension and declination. The properties of these two systems, as reported by \citet{hessels07}, are summarized in Table~\ref{tab:MSP}. M3B is a 2.39 ms MSP, located in binary with a $\sim 1.4$ days circular orbit. Its general radio properties suggest that it is a canonical system and therefore it should be in a binary system with a WD companion. On the other hand, M3D has a spin period of 5.45 ms and it is in a very long and slightly eccentric orbit of about 129 days. The vast majority of binary MSPs in GCs have orbital periods shorter than few days, while just a dozen have orbital periods longer than 10 days\footnote{see \url{http://www.naic.edu/~pfreire/GCpsr.html}}. Therefore M3D likely underwent an anomalous evolution; indeed, binaries with orbital periods longer then 10 days are believed to be formed through an exchange interaction between an isolated NS and a primordial cluster binary \citep{hut92,sigurdsson93}. Its eccentricity, which is likely the result of fly-by encounters with other stars \citep{phinney92,phinney93,bagchi09}, is unexpected for systems formed through the canonical low-mass X-ray binary channel and confirms a non-standard evolution for this system.

Here we report on the secure identification of the companion star to M3B and on a candidate companion to M3D. These companions have been discovered through high resolution near-ultraviolet (near-UV) and optical observations. In Section~\ref{sec:data} we present the data-set we used in this work and the data reduction procedures. In Section~\ref{sec:comM3B} we present the identification and characterization of the companion star to M3B, while in Section~\ref{sec:comM3D} we discuss a possible candidate companion to M3D. Finally, in Section~\ref{sec:conc} we draw our conclusions.

\begin{deluxetable*}{lcc}
\tablecolumns{3}
\tablewidth{0pt}
\tablecaption{Main radio timing
parameters for M3B and M3D\tablenotemark{a}, from \citet{hessels07}.\label{tab:MSP}}
\tablehead{\colhead{Parameter} & \colhead{M3B} & \colhead{M3D}}
\startdata
Right ascension, $\alpha$ (J2000)\dotfill  & 13$^{\rm h}\,42^{\rm m}\,11\fs0871(1)$  & 13$^{\rm h}\,42^{\rm m}\,10\fs2(6)$    \\
Declination, $\delta$ (J2000)  \dotfill  & $28^\circ\,22'\,40\farcs141(2)$   & $28^\circ\,22'\,36(14)\arcsec$  \\
Angular offset from cluster center, $\theta_{\perp}$ (\arcsec) \dotfill & 8.4 & 14(7) \\
Spin period, $P$ (ms)  \dotfill  & 2.389420757786(1) &   5.44297516(6) \\
Orbital period, $P_b$ (days) \dotfill & 1.417352298(2) & 128.752(5) \\
Time of ascending node passage, $T_{asc}$ (MJD) \dotfill & 52485.9679712(6) & 52655.38(4) \\
Projected semi-major axis, $x$ (s) \dotfill & 1.875655(2) & 38.524(4)\\
Eccentricity, $e$ \dotfill & ... & 0.0753(5) \\
MSP mass function, $f \ (M_{\odot})$ \dotfill  & 0.003526842(6) & 0.0037031(8) \\
\hline
\enddata
\tablenotetext{a}{Numbers in parentheses are uncertainties in the last digits quoted.}
\end{deluxetable*}

\section{Observations and DAta analysis} \label{sec:data}

This work is based on a archival data-set of deep, high resolution near-UV and optical observations obtained through the UVIS channel of the Wide Field Camera 3 mounted on the Hubble Space Telescope (GO 12605, PI: Piotto). The data-set is composed of 6 images in the F275W {(near-ultraviolet)} filter with exposure time of 415 s, 4 images in the F336W (U) filter with exposure time of 350 s and 4 images in the F438W (B) filter with exposure time of 42 s. All the images {have been obtained on May 15th 2012 during $\sim5$ hours of continual observations and thus they only cover $\sim15\%$ and $\sim0.16\%$ of the orbits of M3B and M3D, respectively}. The images are dithered by few arcseconds each, in order to avoid spurious effects due to bad pixels and to fill the inter-chip gap. The photometric analysis has been performed with {\rm DAOPHOT IV} \citep{stetson87} adopting the so-called ``UV-route'' as described in \citealt{raso17} (see also \citealt{ferraro97b,ferraro01b,ferraro03c,dalessandro18a,dalessandro18b}). As a first step, about 200 stars have been selected in each image in order to model the point spread function, which has been then applied to all the sources detected at more than $5\sigma$ from the background level. Then, we built a master catalog with stars detected in at least half the near-UV (F275W) images. At the corresponding position of these stars, the photometric fit was forced in all the other frames  by using {\rm DAOPHOT/ALLFRAME} \citep{stetson94}. Using such a near-UV master list, the crowding effect due to the presence of giants and turn-off stars is mitigated and several blue stars like blue stragglers and white dwarfs are recovered. Finally, for each star we homogenized the magnitudes estimated in different images, and their weighted mean and standard deviation have been adopted as the star magnitude and its related photometric error. The instrumental magnitudes have been reported to the VEGAMAG system by cross-correlation with the catalog of the ``{\it The Hubble Space Telescope UV Legacy Survey of Galactic globular clusters}'' \citep{piotto15}, obtained from the same data-set used in this work and publicly available.

The star detector positions have been corrected from geometric distortion following the procedure described by \citet{bellini11}. Then, these positions have been reported to the absolute coordinate system ($\alpha$,$\delta$) using the stars in common with the Gaia DR2 catalog \citep{gaia18}. The coordinate system of this catalog is based on the International Celestial Reference System, which allows an appropriate comparison with the MSP positions derived from timing using solar system ephemerids, being the latter referenced to the same celestial system. The resulting $1\sigma$ astrometric uncertainty is of $\sim 0.1 \arcsec$ in both $\alpha$ and $\delta$.

\section{IDENTIFICATION OF THE COMPANION STAR to M3B} \label{sec:comM3B}

\begin{figure}[t]
\centering
\includegraphics[scale=0.72]{chartB.png}
\caption{$3\arcsec \times 3 \arcsec$ finding chart of the region around the radio position of M3B. The left, middle and right panels are extracted from a F275W, F336W and F438W image, respectively. The red cross is centered on the MSP position and the red circle has a radius $r=0.15\arcsec$. The only star located within this circle is the identified companion to M3B.}
\label{fig:chartB}
\end{figure}

\begin{figure}[h!]
\centering
\includegraphics[scale=0.49]{cmd_M3B.pdf}
\caption{($m_{F275W}$, $m_{F275W}-m_{F336W}$) CMD of M3 obtained from the data-set used in this work. The positions of the companion star to M3B is marked with a red square.}
\label{fig:cmd}
\end{figure}

In order to search for the companion star to M3B, we investigated all the stellar sources detected in a $3\arcsec \times 3 \arcsec$ region surrounding the MSP timing position reported in Table~\ref{tab:MSP}. The stellar source closest to the radio position turned out to be a very blue object, located at $\alpha=13^{\rm h}\,42^{\rm m}\,11\fs0881$ and $\delta=28^\circ\,22'\,40\farcs141$, at only $0.01 \arcsec$ from the radio MSP position. The finding chart of this object in the three different filters is reported in Figure~\ref{fig:chartB}. In the color-magnitude diagram (CMD) this star is located along the red side of the WD cooling sequence, in a region where WDs with a He core are expected to be found (see Figure~\ref{fig:cmd}). The combination of the excellent agreement between the radio and the optical position and the peculiar location in the CMD allows us to safely conclude that the identified WD is the companion star to M3B. Its magnitudes in the three filters are the following: $m_{F275W}=22.45\pm0.05$, $m_{F336W}=22.75\pm0.05$ and $m_{F438W}=23.4\pm0.2$.
Although multiple epoch images are available for each filter, no evidence of photometric variability has been observed for the companion star. While this could be due to the poor and sparse orbital period coverage provided by the available data-set, {we stress that the photometric variability is only rarely observed for degenerate companion stars and is not due to the re-heating of the star by the MSP emitted energy, which is generally negligible, but most likely to pulsations (global stellar oscillations) of the WD itself \citep[e.g.][]{maxted13,kilic15}.}

\begin{figure}[b]
\centering
\includegraphics[scale=0.4]{cmdwdB.pdf}
\caption{Same as in Figure~\ref{fig:cmd} but zoomed into the WD region. As reported in the top legend, the blue curve is a cooling track for $0.55 \, M_{\odot}$ C-O WDs from the {\it BaSTI} database, while the cyan curves are He WD cooling tracks with masses, from left to right, of $0.24 \, M_{\odot}$, $0.23 \, M_{\odot}$, $0.20 \, M_{\odot}$, $0.19 \, M_{\odot}$ and $0.18 \, M_{\odot}$, calculated at the cluster metallicity $(Z\sim0.0005)$ following \citet{istrate14,istrate16}. Points at different cooling ages are highlighted with gray symbols as reported in the secondary legend.}
\label{fig:cmdwd}
\end{figure}

We can now compare the measured magnitudes with those predicted by He WD cooling sequences in order to derive the main physical properties of the companion star. As a first step, we checked the validity of the photometric calibration by comparing the observed sequence of standard WDs with a theoretical cooling model for C-O WDs with masses $M=0.55 \ M_{\odot}$ taken from the {\it BaSTI} database \citep{salaris10}. Absolute magnitudes have been reported to the observed frame by adopting a color-excess $E(B-V)=0.01$, a distance modulus $(m-M)_V=15.07$ \citep{harris10}, and appropriate extinction coefficients for each filter: $A_{F275W}/A_V =1.94$, $A_{F336W}/A_V =1.66$ and $A_{F438W}/A_V =1.33$ \citep{cardelli89,odonnell94}. The corresponding curve is shown in Figure~\ref{fig:cmdwd} and its agreement with the observed WD sequence confirms the accuracy of the adopted photometric calibration and cluster parameters.

In the case of the He WDs, we built a set of theoretical tracks using the new models for extremely low-mass He WD by \citet{istrate14,istrate16}. These models are particularly appropriate for the present case study, since they simulate the entire evolution of systems within the low-mass X-ray binary channel, also including the effects of rotational mixing and element diffusion {and adopting the appropriate cluster metallicity for the secondary stars}. A selection of the obtained cooling tracks is shown in Figure~\ref{fig:cmdwd} (cyan lines).

It is now possible to use the theoretical tracks to constrain the main physical properties of the detected WD such as its mass, surface temperature and cooling age\footnote{The WD cooling age is defined, according to \citet{istrate16}, as the time passed since the proto-WD reached the maximum surface temperature along the evolutionary track.}. To do this, we used an approach similar to that implemented by \citealt{dai17} (see also \citealt{pallanca13a}, \citealt{testa15}). We interpolated all the available models to create a fine grid in the mass range $0.16 \, M_{\odot}$ - $0.35 \, M_{\odot}$, temperature range 9000~K~-~21000~K and cooling age range 0.1~Gyr~-~3~Gyr. Assuming Gaussian photometric errors,  we thus estimated the likelihood of each point of the grid (i.e. of each possible combination of the three parameters) as:
$$
L = \prod_{j} \frac{exp\left[\frac{-\left(m_j - m_j^{mod}\right)^2}{2\delta_j^2}\right]}{\sqrt{2\pi \delta_j^2}}
$$
where the index $j$ runs through the three photometric filters F275W, F336W and F438W, $m_j$ and $\delta_j$ are the observed magnitudes and related errors and $m_j^{mod}$ is the magnitude predicted by the models at that point of the grid (see equation 5 in \citealt{dai17}).

The marginalized 1D and 2D likelihood distributions are presented in the corner plot\footnote{see \url{https://corner.readthedocs.io/en/latest/} \citep{foreman16}} of Figure~\ref{fig:cornerM3B}. For each parameter, the best-fit value, the lower and the upper uncertainties have been estimated as the $50^{th}$, $16^{th}$ and $84^{th}$ percentile of its likelihood distribution, respectively. We therefore found that the He WD has a mass $M_{COM}~=~0.19~\pm~0.02~ \ M_{\odot}$, a cooling age of $1.0^{+0.2}_{-0.3}$ Gyr and an effective temperature of $T=12\pm 1\cdot10^3$ K. The derived cooling age is consistent with the MSP spin-down age ($>1.1$~Gyr) estimated by \citet{hessels07}.
\begin{figure}[b]
\centering
\includegraphics[scale=0.45]{cornerM3B.pdf}
\caption{Constraints on the mass, cooling age and surface temperature of the companion star to M3B. The 1D histograms show the likelihood marginalized distributions for each of the three parameters and the blue solid and black dashed lines are, respectively, the $50^{th}$, $16^{th}$ and $84^{th}$ percentiles of each distribution, that have been used as estimates of the best-fit value of each parameter and their related uncertainty. The contours in the 2D histograms correspond to $1\sigma$, $2\sigma$ and $3\sigma$ levels and the best values for each parameter are marked with the blue point and lines. The text at the top  reports the derived mass, cooling age and temperature values.}
\label{fig:cornerM3B}
\end{figure}
From the best-fit model we have also inferred that the proto-WD phase\footnote{{ It is the phase following the mass-transfer stage, when the He core contracts at an almost constant luminosity before starting its cooling phase \citep[see][]{istrate14,istrate16}}.} lasted for $1.0^{+0.1}_{-0.5}$ Gyr and that this star is composed of a core with a mass of about $0.18 \ M_{\odot}$ and a thin envelope with mass of about $0.01 \ M_{\odot}$. The total He mass is around $0.187 \ M_{\odot}$, while the H mass is only around $0.003 \ M_{\odot}$. Finally, its central density and  temperature are around $1.3 \cdot 10^{5}$~g/cm$^{-3}$ and $2\cdot 10^{7}$~K, respectively.

{{The companion star parameters just derived can be used to investigate the physical properties of its progenitor star.} We used the {\rm PARSEC} evolutionary tracks \citep{bressan12,bressan13} to study the evolution of the He core of isolated stars with different masses and ages at the cluster metallicity. Assuming a cluster stellar population age of $12.5\pm0.5$ Gyr \citep{dotter10} and using the derived cooling age and proto-WD phase duration, we can estimate that the mass-transfer stopped (i.e. the Roche-Lobe detachment occurred) when the cluster had an age around $10.5\pm0.8$ Gyr. {Within this age range, only stars in the mass range $0.82 \ M_{\odot} - 0.85 \ M_{\odot}$ have grown a He core with a mass comparable with that derived for the companion to M3B (see left panel of Figure~\ref{fig:massacore}). On the other hand, at an age $t=10.5\pm0.8$ Gyr and at the cluster metallicity, the mass of a star at the main sequence turn-off is $0.81^{+0.01}_{-0.02} \ M_{\odot}$ and stars as massive as $0.82 \ M_{\odot} - 0.85 \ M_{\odot}$ are already evolved toward the red giant branch. Indeed, as shown in the evolutionary tracks plotted in right panel of Figure~\ref{fig:massacore}, stars with mass in the range $0.82 \ M_{\odot} - 0.85 \ M_{\odot}$ have grown a $0.19\pm0.02 \ M_{\odot}$ He core at the base of the red giant branch. By assuming that the mass-transfer phase lasted approximately $\sim1$ Gyr, we can infer that the it started just after the star left the main sequence stage and therefore the bulk of the mass-transfer essentially occurred during the sub-giant branch phase, where the star is expected to expand as a consequence of its canonical evolution and so is able to fill its Roche-Lobe. Therefore the observational properties of the M3B companion measured here appear to be fully consistent with a suitable scenario for the formation of the MSP.}}

\begin{figure}[b!]
\centering
\includegraphics[scale=0.32]{masscore2.png}
\includegraphics[scale=0.32]{hr.png}
\caption{{{\it Left Panel:} He core mass as a function of the stellar mass  as predicted by \citet{bressan12,bressan13} evolutionary tracks. The black solid curve and the light gray shaded area represent the values for an age of $10.5\pm0.8$ Gyr. The horizontal line (and dark gray band) marks the mass of the He WD companion to M3B (and its related uncertainty) as derived in Section~\ref{sec:comM3B}. {\it Right Panel:} evolutionary tracks for different stellar masses as reported in the top-left legend. The red region of the tracks highlights the phase where the stars have grown a He core with a mass comparable with the one measured for the companion to M3B at an age of $10.5\pm0.8$ Gyr (corresponding to the mass-transfer end, i.e. the Roche-Lobe detachment phase). The blue shaded area marks the region of the tracks 1 Gyr before the Roche-Lobe detachment, when the mass-transfer probably started.}}
\label{fig:massacore}
\end{figure}

The He WD mass here obtained ($M_{COM}$), combined with the MSP mass function ($f$) derived from radio timing (see Table~\ref{tab:MSP}) can be use to constrain the orbital inclination angle $i$ and, most importantly, the mass of the NS ($M_{NS}$). Indeed these quantities are related by the following equation:
\begin{equation}
f(M_{NS}, M_{COM}, i) = \frac{(M_{COM}\sin{i})^3}{(M_{NS}+M_{COM})^2}
\end{equation}
We used the affine-invariant Markov Chain Monte Carlo (MCMC) ensemble sampler {\rm emcee\footnote{\url{https://emcee.readthedocs.io/en/stable/}}} \citep{foreman13} to constrain $M_{NS}$ and $i$. We set a Gaussian prior on $M_{NS}$, centered at $1.4 \ M_{\odot}$, which is the mass typically measured for NSs in binary MSPs \citep{ozel16}, and with a standard deviation of $0.5 \ M_{\odot}$, {large enough to include the observed NS mass distribution \citep{antoniadis16}}. $M_{NS}$ is sampled in the range $0.5 \ M_{\odot}$ - $2.5 \ M_{\odot}$. On the other hand, we set an uniform prior on the distribution of $\cos{i}$ in the range 0 - 1. The results are presented in Figure~\ref{fig:mpsrB}. The best value for the NS mass is $M_{NS}=1.1\pm 0.3 \ M_{\odot}$, {thus suggesting that this system hosts a low-mass NS, although the value is still compatible with the typical NS masses measured for these kind of systems. Results do not change if wider NS mass distributions are used}. The probability distribution of the inclination angle is shaped as a truncated Gaussian and clearly shows that this system is observed almost edge-on. We therefore assumed that the best value for the inclination angle corresponds to the maximum in the probability distribution and its lower uncertainty to the $16^{th}$ percentile of an identical but symmetric probability distribution. Doing so we have estimated the inclination angle to be $i=89^{+1}_{-26}$ degrees. { All the physical properties of the binary here derived are summarized in Table~\ref{tab:comMSP}.}
\begin{figure}[h]
\centering
\includegraphics[scale=0.6]{corner_mpsrB.pdf}
\caption{Constraints on the mass of the NS and on the orbital inclination angle of M3B. The 1D histograms are the marginalized probability distributions of the two parameters, where the solid blue and black dashed lines are the best values and their related uncertainties (see text). The bottom left panel is the joint 2D posterior probability distribution and the contours corresponds to $1\sigma$, $2\sigma$ and $3\sigma$ confidence levels.}
\label{fig:mpsrB}
\end{figure}

\section{A He WD ORBITING M3D TOO?}\label{sec:comM3D}

\begin{figure}[h]
\centering
\includegraphics[scale=0.16]{chartD.png}
\caption{Left panel: $15\arcsec \times 18\arcsec$ chart of the region surrounding M3D, obtained from a F275W image. The black box is centered on the MSP position and corresponds to the error box quoted in \citet{hessels07}. The red circle indicates the position of the candidate companion. Right panel: same as in the left panel, but zoomed into the position of the candidate companion.}
\label{fig:chartD}
\end{figure}

\begin{figure}[h!]
\centering
\includegraphics[scale=0.35]{cmd_M3D.pdf}
\includegraphics[scale=0.35]{cmdwdD.pdf}
\caption{{{\it Left panel:} same as in Figure~\ref{fig:cmd}. The position of the candidate companion star to M3D is marked with a large red square, while the positions of all the other stars within the investigated area is marked with smaller red squares. {\it Right panel:} same as in Figure~\ref{fig:cmdwd} but for the candidate companion to M3D.}}
\label{fig:cmdD}
\end{figure}

The timing solution of M3D reported by \citet{hessels07} provides the celestial position of this binary affected by a modest uncertainty ($0.6\arcsec$) in $\alpha$ and a large uncertainty ($14\arcsec$) in $\delta$. Therefore the search for the optical counterpart to this system is challenging. We carefully investigated all the stellar sources within and nearby the position error box: {this region of interest is centered on the best MSP position (see Table~\ref{tab:MSP}) and is as large as the $3\sigma$ uncertainty in $\alpha$ and $2\sigma$ uncertainty in $\delta$. We only found a possible candidate in a position marginally compatible with the radio one (see Figure~\ref{fig:chartD} and Figure~\ref{fig:cmdD}). In fact, all the stars detected within the investigated area likely belong to the canonical evolutionary sequences but one source located again on the red side of the WD cooling sequence, in a position compatible with that of the He WDs}. This candidate counterpart is located at $\alpha=13^{\rm h}\,42^{\rm m}\,10\fs3041$ and $\delta=28^\circ\,22'\,44\farcs786$. The right ascension is shifted by $1.5\arcsec$ from the radio value, which is larger than the combined radio uncertainty and optical astrometric precision.  Its observed magnitudes are: $m_{F275W}=23.06\pm0.08$, $m_{F336W}=23.35\pm0.08$ and $m_{F438W}=24.1\pm0.3$.
Following the same method used for M3B and presented in Section~\ref{sec:comM3B}, we found that this star has a mass $M_{COM}=0.22 \pm 0.02 \ M_{\odot}$, a cooling age of $1.1^{+0.7}_{-0.6}$ Gyr and an effective temperature of $13\pm 2 \cdot 10^{3}$ K. Using the MSP mass function (Table~\ref{tab:MSP}) we estimated the NS mass to be $M_{NS}=1.3 \pm 0.3 \ M_{\odot}$ and the orbital inclination angle to be $i=72\pm16$ degrees (see Table~\ref{tab:comMSP}). Again, the $M_{NS}$ value would be in agreement with the typical values observed for binary MSPs.
We tried to establish phase-connection of the MSP timing solution using the available radio data and fixing the MSP position to that of the candidate counterpart. Unfortunately, this did not lead to an improvement of the timing solution obtained by \citet{hessels07}.
Given all this, we cannot solidly confirm that the detected He WD is the optical counterpart to M3D, {which could be still under the detection threshold. Furthermore, the peculiar evolution that this system likely underwent implies that the companion star might not be a classical He WD. However it is worth noting that a He WD has been identified orbiting B1620$-$26 in M4, the only similar MSP with an optical counterpart to date \citep{sigurdsson03}.} Future radio observations and timing analysis are needed to improve the position measurement of this object.

\begin{deluxetable*}{lcc}
\tablecolumns{3}
\tablewidth{0pt}
\tablecaption{Physical properties of the binaries M3B and M3D as derived in Section~\ref{sec:comM3B} and ~\ref{sec:comM3D}. \label{tab:comMSP}}
\tablehead{\colhead{Parameter} & \colhead{M3B} & \colhead{M3D?}}
\startdata
Companion mass, $M_{COM} \ (M_{\odot})$\dotfill  & $0.19\pm0.02$ & $0.22\pm0.02$    \\
Effective temperature, $T$ ($10^3$ K) \dotfill & $12\pm1$ & $13\pm2$ \\
Cooling age, Age (Gyr) \dotfill & $1.0^{+0.2}_{-0.3}$ & $1.1^{+0.7}_{-0.6}$ \\
Neutron star mass, $M_{NS} \ (M_{\odot})$\dotfill  & $1.1\pm0.3$ & $1.3\pm0.3$    \\
Inclination angle, $i$ (deg) \dotfill & $89^{+1}_{-26}$ & $72\pm16$ \\
\hline
\enddata
\end{deluxetable*}

\section{CONCLUSIONS}\label{sec:conc}

We used deep and high resolution images obtained at near-UV and optical wavelengths to search for the companion stars to the binary MSPs in the GC M3. By exploiting the ``UV route'' to dilute the crowding issues in the cluster center and increase the sensitivity to blue/hot stars, we have been able to firmly identify the companion star to the canonical MSP M3B and find a candidate counterpart to the anomalous (long period and mild eccentricity) system M3D.
The companion star to M3B turned out to be a WD with a He core, as expected from the canonical formation scenario. Interestingly, despite the fact that this cluster hosts a stellar population with an intermediate metallicity, the companion is an extremely low-mass object, with a mass of about $0.19 \ M_{\odot}$. Indeed, the lower is the metal content of the secondary stars, the larger is expected to be the minimum mass of the WD remnants. This is due to the fact that low metallicity stars have shorter evolutionary timescales and smaller radii and therefore their Roche Lobe is filled (i.e. the mass-transfer starts) in a more advanced stage of their evolution, when the He core is grown more massive than it would have for a more metal-rich system \citep{istrate16}. Our mass measurement is indeed close to the minimum possible mass produced by the adopted models at the cluster metallicity. This stresses the importance of the study of extremely low-mass WD systems, with special care to the physical processes occurring during the evolution. In fact, the models we used take into account effects like rotational mixing and element diffusion. Models not including these effects are characterized by bluer cooling tracks that would have not been able to reproduce the observed magnitudes of the companion or, in the case they do, the resulting companion mass would have been so small that the corresponding NS mass becomes unreasonable (i.e. $<1 \ M_{\odot}$). {We have also shown that the progenitor of this WD was likely a $\sim0.83 \ M_{\odot}$ star which filled its Roche-Lobe after leaving the main sequence, thus implying that the bulk of the mass-transfer activity occurred during the sub-giant branch phase. All the derived physical properties of the companion star, combined with the information obtained through radio timing, allowed to infer that this binary is observed almost edge-on and probably hosts a low-mass NS with a mass around $\sim 1.1 \ M_{\odot}$.}

In the case of the candidate companion star to M3D, we have identified a He WD at a position marginally compatible with the highly uncertain radio one. Therefore the association between this degenerate object and the MSP cannot be confirmed yet. This WD is again a low-mass object with a mass around $0.22 \ M_{\odot}$ and a cooling age of $\sim1$~Gyr

{\citet{tauris99} discussed the correlation between the masses of the WD companion stars and the orbital periods of the binary MSPs (the so-called ``TS99'' relation; see also \citealt{istrate14} for a more recent investigation on this). According to this relation, the $\sim1.4$~days orbit of M3B implies a companion star with a mass of $\sim0.21 \ M_{\odot}$, fully compatible, within the uncertainties, with the mass value derived in this work. On the other hand, the long $\sim 129$ days orbit of M3D implies a companion star with a mass around $\sim 0.35 \ M_{\odot}$, a value significantly larger than the one here derived for its candidate companion star. This could suggests that the proposed optical counterpart is not the real companion star, even though its mass is compatible with the measured MSP mass function if a typical NS mass is assumed. If this WD is truly the companion star to M3D, the discrepancy between the measured mass and the one predicted by the TS99 relation could be explained by the formation of this system through an exchange interaction occurred after the NS recycling phase. Such an exchange, however, is expected to produce highly eccentric binaries \citep[see][]{prince91,freire04,lynch12}, while only a mild eccentricity is measured for this system.}

\acknowledgments
{We thank the anonymous referee for the careful reading of the manuscript}. This research is part of the scientific project Cosmic-Lab at the Department of Physics and Astronomy at Bologna University.

\vspace{5mm}
\facilities{HST(WFC3)}
\software{DAOPHOT \citep{stetson87}, {\rm emcee} \citep{foreman13}, {\rm corner.py} \citep{foreman16}}

\section{}

\textit{Research Notes of the \href{https://aas.org}{American Astronomical Society}}
(\href{http://rnaas.aas.org}{RNAAS}) is a publication in the AAS portfolio
(alongside ApJ, AJ, ApJ Supplements, and ApJ Letters) through which authors can
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The astronomical community has long faced a challenge in disseminating
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There have generally been few options available for sharing works in progress,
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Submissions to RNAAS should be brief communications - 1,000 words or fewer
\footnote{An easy way to count the number of words in a Research Note is to use
the \texttt{texcount} utility installed with most \latex\ installations. The
call  \texttt{texcount -incbib -v3 rnaas.tex}) gives 57 words in the front
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option is by copying the words into MS/Word, and using ``Word Count'' under the
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Authors are expected to follow the AAS's ethics \citep{2006ApJ...652..847K},
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\begin{figure}[h!]
\begin{center}
\includegraphics[scale=0.85,angle=0]{aas.pdf}
\caption{Top page of the AAS Journals' website, \url{http://journals.aas.org},
on October 15, 2017.  Each RNAAS manuscript is only allowed one figure or
table (but not both). Including the
\href{http://journals.aas.org//authors/data.html\#DbF}{data behind the figure}
in a Note is encouraged, and the data will be provided as a link in the
published Note.\label{fig:1}}
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\acknowledgments

Acknowledge people, facilities, and software here but remember that this counts
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It's that time of year when the days are longer, and it becomes easier to do something about the carpet stains that may have built up, dust and stale air that have built up during the last few weeks and, perhaps, months. You can throw open all of the windows and let in the fresh air without freezing. Now, get ready to give your home a good spring and summer cleaning.
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text:
Q: How to solve QPixmap::fromImage memory leak? I have a problem with Qt.
Here is a part of code that troubles me:
    void FullScreenImage::QImageIplImageCvt(IplImage *input)
{
    help=cvCreateImage(cvGetSize(input), input->depth, input->nChannels);
    cvCvtColor(input, help, CV_BGR2RGB);
    QImage tmp((uchar *)help->imageData, help->width, help->height, help->widthStep, QImage::Format_RGB888);
    this->setPixmap(QPixmap::fromImage(tmp).scaled(this->size(), Qt::IgnoreAspectRatio, Qt::SmoothTransformation));
    cvReleaseImage(&help);
}

void FullScreenImage::hideOnScreen() {
    this->hide();
    this->clear();
}

void FullScreenImage::showOnScreen(IplImage *slika, int delay) {
    QImageIplImageCvt(slika);
    this->showFullScreen();
    if(delay>0)
 QTimer::singleShot(delay*1000, this, SLOT(hideOnScreen()));
}

So, the method showOnScreen uses private method QImageIplImageCvt to create QImage from IplImage (which is used by the OpenCV), which is then used to create QPixmap in order to show the image in full screen. FullScreenImage class inherits QLabel.
After some delay, the fullscreen picture should be hidden, so I use QTimer to trigger an event after some delay. The event handler is the hideOnScreen method which hides the label and should clear the memory.
The problem is the following:
Whenever I call QPixmap::fromImage, it allocates the memory for the pixmap data and copies the data from QImage memory buffer to the QPixmap memory buffer. After the label is hidden, the QPixmap data still remains allocated, and even worse, after the new QPixmap::fromImage call the new chunk of memory is allocated for the new picture, and the old data is not freed from memory. This causes a memory leak (cca 10 MB per method call with my testing pictures). How can I solve that leak?
I've even tried to create a private QPixmap variable, store pixmap created by the QPixmap::fromImage to it, and then tried to call its destructor in hideOnScreen method, but it didn't help.
Is there a non-static way to create QPixmap from QImage? Or even better, is there a way to create QPixmap directly from IplImage* ?
Thank you in advance for your answers.

A: There is no way to create QPixmap directly from IplImage* (and also not from cv::Mat). However, your solution there is to refrain from writing everything into one line and work with a pointer that you free yourself.
e.g.:
if (this->mypixmap)
    delete this->mypixmap;
this->mypixmap = new QPixmap(QPixmap::fromImage(tmp).scaled(this->size(), Qt::IgnoreAspectRatio, Qt::SmoothTransformation));
this->setPixmap(this->mypixmap);

Don't forget to set mypixmap(NULL) in the constructor.

A: You should be able to use QPixmap::loadFromData to create a QPixmap directly. So something like the following might work:
QPixmap p;
p.loadFromData((uchar *)help->imageData, help->width * help->height);

Without knowing anything about OpenCV or IplImage, I can't guarantee that the above snippet is correct, but hopefully it starts you down the right path.

A: I had a similar problem, however my code was different so its not worth me putting here.  Taking your code and merging with my method would give you:
void FullScreenImage::QImageIplImageCvt(IplImage *input)
{
    help=cvCreateImage(cvGetSize(input), input->depth, input->nChannels);
    cvCvtColor(input, help, CV_BGR2RGB);
    QImage* tmp = new QImage((uchar *)help->imageData, help->width, help->height, help->widthStep, QImage::Format_RGB888);
    this->setPixmap(QPixmap::fromImage(*tmp).scaled(this->size(), Qt::IgnoreAspectRatio, Qt::SmoothTransformation));
    delete tmp;
    cvReleaseImage(&help);
}

A: Using the overloaded method solved the issue for me:
QPixmap::fromImage(const QImage && image,..)

You can call it with:
QPixmap::fromImage(std::move(tmp))

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A farm wedding would be just right for flowers mixed with fruit. This loose arrangement includes citrus ranunculus and geraniums.
Oh – love this! I had my florist include fruit in the centerpieces at my wedding reception. She included lemons, limes, pears, apples and plums. Beautiful!


"This is the next critical wave of creating a democratic economy. In the 1940s, as a nation we made an imperfect but concerted drive to spread homeownership to the point where two-thirds of Americans now own their own home," Kelly adds. "I think broadening business ownership would be transformative and potentially a part of the answer to the problem of wealth inequality." Read full article.


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