text:
Doctors joining nurses' strike
23 Jun 2020 at 07:56hrs | Views
JUNIOR doctors have threatened to go on strike, joining the industrial action by nurses that started last week citing deteriorating working conditions, which will negatively affect the country's battle against the growing coronavirus pandemic.
Nurses have been picketing since Wednesday last week, demanding salaries in United States dollars after rejecting an offer to hike their earnings by 50% and US$75 allowances.
They said soaring inflation, which is the world's
highest at 785,55% as of May, has drastically reduced the value of their Zimdollar salaries and has seen prices of goods rising almost daily.
The situation is reminiscent of the hyperinflation era of 2008, when prices changed several times daily to keep up with inflation, which eventually topped 500 billion percent.
Junior doctors could soon join the strike, with officials saying they were "in a similar situation" to that of nurses.
"We struggle to get fuel when we are on call. Many stations are selling in US dollars, so we are now incapacitated," an official with an association representing the doctors told NewsDay, but preferred anonymity for fear of reprisals.
Last year, the doctors went on strike for over four months over pay and poor working conditions, paralysing the country's healthcare sector.
The strike only ended in January this year when they accepted an offer by Econet founder and telecoms billionaire Strive Masiyiwa, who set up a $100 million fund to pay up to 2 000 doctors a subsistence allowance of US$300 a month at the time to help them with transport and living costs.
The programme was for six months. Nurses say they will not return to work until their demands are met, a situation confirmed by Mpilo Central Hospital acting clinical director Xolani Ndlovu yesterday.
"Most of the qualified nurses are at home, they did not report for duty. They vowed that they will not come back until government addresses their demands. We only have a skeleton staff most of them being nurses on probation. We also have doctors and some have already started threatening to join the strike soon," Ndlovu said, adding the hospital was dealing with emergencies only.
Speaking to NewsDay yesterday, Zimbabwe Professional Nurses Union president Robert Chiduku said the health workers would not bow down to pressure.
"We heard reports from our distressed colleagues in Mutare and other parts of the country, who are being victimised for engaging in the strike. Our message to government is that you do not satisfy hunger of your child by whipping him or her. You simply attend to the needs and provide the food then life goes on," he said.
"We are prepared for any form of reign of terror because this is not the first time nurses have been victimised. It is senseless to victimise the hungry and naked workers. We will not call off the strike until our salaries are paid in United States dollars."
President of the Zimbabwe Nurses Association (Zina), Enock Dongo, said nothing official had been communicated yet and urged government to urgently address their concerns.
"Patients are getting stranded and the situation is worsening. They need to resolve this impasse as a matter of urgency," he said.
Dongo said he had held an informal meeting with the Health Services Board to update them on the situation.
"It was an informal meeting, where a few issues were clarified, but we are still waiting for the concrete resolutions," he said.
Dongo also said the situation was being made worse due to COVID-19 and demand for more staff to manage that area.
Stakeholders called on the government to resolve the situation, but Health minister Obadiah Moyo has legal troubles of his own.
He was arrested last Friday on allegations of corruption involving a US$60 million deal to procure COVID-19 test kits and equipment. A Harare magistrate granted him $50 000 bail on Saturday.
The Senior Hospital Doctors Association also said its members were overwhelmed and pleaded with the government to act.
"The situation at the hospitals is now dire. There is no care available as health workers cannot afford to come to work anymore," a senior doctor said.
"As senior doctors, we condemn the looting of funds meant for the COVID-19 fight and for capacitating our hospitals. We call upon the government to act."
The Community Working Group on Health (CWGH) urged the government and the striking health workers to find each other to avoid further plunging the country's health sector into the doldrums.
"Under normal situations, salaries for civil servants are negotiated under the Tripartite Negotiating Forum, which comprises employees, employers and government representatives.
"The way the increment was announced and the so-called 'clarifications' that followed showed that this was a knee-jerk reaction to pre-empt a protest that was pending," CWGH executive director Itai Rusike said, adding there was need for proactive thinking by the leaders to address issues of national concern.
He said CWGH believed health workers' grievances were genuine and required urgent attention. He also condemned the arrest of some of the striking workers.
"Threats or coercion of any form will further deepen the mistrust that exists between government and the workers. We believe re-engagement and dialogue are the panacea to any dispute," Rusike said.
As a stop-gap measure, Health acting permanent secretary Gibson Mhlanga has since written to the Defence ministry requesting support for the paralysed health institutions.
In a letter addressed to Defence secretary Mark Grey Marongwe, Mhlanga said medical personnel from the Zimbabwe Defence Forces would augment coverage for emergencies and provision of patient care during the absence of nurses.
"We will be calling upon your health services personnel to assist in the hotspots at the central hospitals as requested by the chief executive officers and provincial medical directors of the affected institutions. Your assistance in this matter is greatly appreciated," he wrote.
Critical departments like Mbuya Nehanda Parirenyatwa's maternity wing had skeletal staff to manage the patients, most of whom were turned away.
A source at Sally Mugabe Central Hospital said the hospital was now in a dire situation as many patients were turned away.
"All departments are in serious trouble," the source said.
Chitungwiza nurses, who had largely ignored the strike call, have now joined, with only students and senior staff on duty.
The situation was dire at Masvingo General Hospital, where all nurses did not report for duty except for those in supervisory roles.
At Chimhanda Hospital in Shamva, nurses gathered at the institution early in the morning and agreed to join the strike.
Public hospitals in Gweru, Mutare and Kwekwe were similarly affected.
More on: #Doctors, #Nurse, #Strike
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... As we tried adding the DPUB-ARIA vocab to EPUB 3.1, and the response we got from the EPUB community was "What about the rest of our terms?"
... From an accessibility perspective DPUB-ARIA is valuable, but we are unsure how to move forward. We don't want to keep flip-flopping.
Ivan: It would theoretically possible to say that we keep DPUB-ARIA for accessibility terms and use another method for non-a11y terms. But, this is not really a viable option from an authoring persepctive.
Micheal: Would a structured extensibibility mechanism be helpful?
... This would mean not going necessarily building it through the ARIA WG. ARIA has been involved in some discussion in how it should be involved in HTML. This has been in brought to TAG.
Micheal: In ARIA, the concept of implicit ARIA semantics exists. A different mechanism would still perhaps have a mapping.
rich: This is the first I've heard of this problem. You've taken a lot of ARIA resources to make this happen.
... We have written the mappings, and it's really close to CR. Clearly there are other issues that haven't been addressed.
ivan: This question has been asked many times. We have asked about the extension mechanism numerous times. This is not new.
Ivan: Will the WG accept that?
Tzviya: If I add terms, and there's no mapping, does it validate? what happens to native semantics?
Rich: I think what we need to do is state in the mapping guide that anything with doc- prefix is not mapped.
Janina: Nervous that some of the problem is in the process. If we can improve process to make this doable, then that should be what solves the problem.
... You're looking at semantics that don't have universal applicability, but there is a definite need.
... Dealing with a broader W3C issue.
... if we want to have a separate document tomorrow with no mappings, do we have a mechanism?
mgylling: anything with a doc- prefix that is not mapped is OK? Does that essentially mean that we define doc-*?
rich: if you don't need the WG to do mappings, great. I would prefer not to look at any values.
Markus: DPUB-ARIA is not bound to ARIA 1.1, correct?


Magnolia Mansourkia Mobley is the founder of boutique consulting firm LegalMatters, LLC where she helps clients with legal, privacy and cyber security policy needs. Focusing primarily on venture backed, small/medium sized technology businesses, she designs practical legal and data protection programs as a mechanism to fuel growth, increase brand trust and maximize brand value. She specializes in establishing legal programs, risk mitigation strategies and board advisory services. Her data protection expertise includes emerging issues related to artificial intelligence, IoT devices, autonomous vehicles and the EU General Data Protection Regulation.
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As Chief Privacy Officer, she created a comprehensive data protection program, including policy implementation, product development, incident response and legislative/public policy matters. She led the development and patenting privacy interfaces designed to achieve transparency and innovation in consumer choice features. Her customer centric approach was directly correlated to and widely credited with increasing customer engagement and revenue growth.
Previously, Ms. Mobley served as Vice President, Assistant General Counsel and Chief Privacy Counsel for Verizon Communications where she was responsible for privacy strategy and compliance across Verizon's diverse business units. Her leadership was instrumental in helping Verizon repeatedly secure a coveted place among the top 20 companies in the "Most Trusted Companies for Privacy" - as ranked by independent TRUSTe/Ponemon Institute surveys. Ms. Mobley has a proven track record in the development of best in class consumer privacy programs including crafting compliance tools, implementing policies and best practices and advocacy before state and federal regulators on privacy, security and other Internet policy matters.
Ms. Mobley is a Certified Information Privacy Professional (CIPP/US), a frequent speaker on legal compliance in the technology space and cutting edge privacy issues. She is a member of the bar in Maryland and the Fourth Circuit.
She lives in Great Falls, Virginia with her husband and three daughters.
What Is Your Path to the CPO Title (or Beyond) and How Will You Get There?
Real Privacy Out of Artificial Intelligence?


A (triathlon) involves three separate events: swimming, biking, and running. If you like to be active outdoors, you might do all three of these things regularly. Participating in a triathlon involves competing against other young athletes in a swimming race, a biking race, and a running race. Lots of adults enjoy participating in triathlons, and kids might find them fun, too. Before getting out there to do a triathlon, you need to start a training program to get into shape. As you work to prepare, be very careful about how much exercise you get every day. It's important not to over-train your body because this is when injuries might occur.
Participating in a triathlon is all about endurance. You will need strength and energy to get through each of the three events.
Successful triathletes understand an important concept called pacing. Pacing involves starting a race and making sure that you can finish strong without having to stop because you are too tired. This means that you don't want to expend all of your energy at the beginning: Hold back a bit so you have enough energy for the end of the race.
Triathlon training also gives you practice switching between the different events. A training exercise might involve running for five minutes and then biking for five minutes, switching back and forth several times.
Don't over-train, because this can keep you from your fitness goals. Some training days should be easier, and some should be harder. Take at least one day off each week to give your body a chance to recover.
Everyone needs to exercise for good health. In fact, the minimum recommendation for kids' fitness is 60 minutes of exercise every day. But as you train for a triathlon, you have a special goal in mind. Make sure to stretch your muscles to warm up before you begin to exercise to help prepare your body and prevent injury. When you finish training for the day, cool down to help your muscles recover.
Have fun while you train. Your workout sessions should be enjoyable as you work to perform at your best.
Healthy eating will help make sure that you have the energy you need to train. You will need plenty of complex carbohydrates, lean protein, and fresh fruits and vegetables to give your body the nutrients and energy it needs.
Complex carbohydrates give your body energy for training. Choose whole grains whenever possible because they are healthier. Fresh fruits and vegetables will give you energy, too. They also have vitamins and minerals that your body needs to be strong and healthy. Stay away from foods that are high in fat and sugar; these foods usually don't have a lot of nutrients.
Protein helps make your muscles strong. Choose proteins such as skinless poultry, fish, and other lean cuts of meat. Nuts, seeds, and beans are also good sources of protein.
Anyone training for a triathlon needs to pay special attention to their overall health and fitness. Getting enough sleep is one important thing you need to do. Kids between the ages of 6 and 13 need between nine and 11 hours of sleep every night, and kids age 14 and older need between eight and ten hours of sleep.
As you prepare for a race, make sure you are having fun and enjoying the entire process. Mental preparation will help you stay positive and enthusiastic about participating in a triathlon.


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CSO's 2015 Mobile Security Survival Guide
5 steps to more mobile-security-savvy employees
NotCompable sets new standards for mobile botnet sophistication
CSO50 winners announced
Mobile malware up 75 percent in 2014
Mobile users encountered malware 75% more often in 2014 compared to 2013
By Maria Korolov
Contributing Writer, CSO |
CSO staff
Mobile users encountered malware 75% more often in 2014 compared to 2013, according to a new report from San Francisco-based mobile security firm Lookout, Inc.
The mobile malware encounter rate was 7% last year, up from 4% in 2013, largely due to the proliferation of new ransomware campaigns such as ScarePakage.
"We were expecting an increase, but not of this magnitude," said Aaron Cockerill, the company's vice president of enterprise products.
[ Take this mobile device management course from PluralSight and learn how to secure devices in your company without degrading the user experience. ]
And the threats aren't just more common. They are also far more sophisticated and increasingly dangerous from an enterprise perspective, he said.
"We've seen a significant increase in both the frequency and sophistication of attacks that would truly represent a concern for the enterprise, like exploits that would let the bad guys get access to corporate networks," he said. "We also saw a greater prevalence and sophistication of applications that enable rooting or jail breaking the device."
For enterprises in particular, the top security threats associated with mobile devices are loss of sensitive data and illicit access to corporate networks.
"The threats that we found targeted both of these issues," Cockerill said.
More on mobile security:
Best Android antivirus? The top 10 tools
Best Android security app? Why you're asking the wrong question
3 simple steps to hack a phone (includes video)
Five new threats to your mobile security
Five things to consider for a mobile security policy
The best mobile VPNs for the enterprise and how to evaluate them
Mobile phishing – same attacks – different hooks
Security on the move: protecting your mobile workforce
The report, which was based on aggregated data from Lookout's over 60 million global users, also said that more than 4 million Android users in the US encountered ransomware, with some victims forced to pay as much as $500 to unlock their devices.
According to Jeremy Linden, the company's senior security product manager, malware typically gets onto devices through drive-by downloads from infected websites, and through malicious links in spam emails.
For the most part, the infections target Android devices.
Windows phones? Not so much.
"Anecdotally, the word is that this platform isn't popular enough to inspire any malware creators to write stuff for it, but that might change in the future," Linden said. "Just like BlackBerry."
The Apple iOS platform is less attractive to malware writers because of the curated app store and walled garden architecture.
"We've seen a couple of iOS threats that popped up late last year, like WireLurker, but our telemetry shows that these threats are not in any way significant as far as prevalence, and limited to specific geographies like China," Linden said. "And due to the fact that they only work on jailbroken devices, it's hard to see the kind of prevalence as we see on Android devices in the U.S."
However, that doesn't necessarily mean that enterprises should assume iPhones are completely secure just because there are fewer attacks.
"The nature of the attacks that we see on iOS tend to be more targeted and, as a result of being more targeted, they're less prevalent from a broad numbers game," said Cockerill.
So if a company is targeted, the attack could come over that vector as well as anywhere else. Plus, users are less aware of iOS risks, so are less prepared to respond if something does happen.
Maria Korolov has been covering emerging technology and emerging markets for the past 20 years.

redpajama_set_name: RedPajamaCommonCrawl


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text:
Jan van Kessel Młodszy także Jan van Kessel II lub III (ur. 23 listopada 1654 w Antwerpii, zm. 1708 w Madrycie) - flamandzki malarz portrecista, aktywny głównie w Madrycie.

Był synem i uczniem Jana van Kessela starszego, malarza martwych natur, zwierząt i girland kwiatowych. Pod koniec lat 70. XVII wieku osiadł na stałe w Madrycie i w 1686 został nadwornym malarzem Karola II Habsburga, króla Hiszpanii. Malował oficjalne portrety i sceny rodzajowe łącząc cechy flamandzkiego malarstwa portretowego z kolorystyką i techniką charakterystyczną dla sztuki hiszpańskiej.

W zbiorach Muzeum Narodowego w Warszawie znajduje się jego obraz Portret rodzinny w ogrodzie (nr inw. M.Ob.813).

Przypisy

Bibliografia

Linki zewnętrzne

Urodzeni w 1654
Zmarli w 1708
Flamandzcy malarze barokowi
Flamandzcy malarze nadworni
Malarze nadworni Karola II Habsburga

redpajama_set_name: RedPajamaWikipedia


Identify if it is really stress that you are feeling or could it be pressure or anxiety?
Take personal responsibility for how you are feeling avoid blaming others.
Control your self-talk – are you being a 'Champion' or a 'Victim'? Is the situation really so difficult or are you reverting back to past situations? How would the situation be different if you viewed it as a glass half full?
Be innovative/creative in your thinking. Don't focus on everything being a problem but ask yourself what would the solution look like.
Relax in your lunch break even if its just 10 minutes. Change your environment, stretch or go for a walk to aid relaxation and to get a different perspective.
Avoid putting too much pressure on yourself to do things perfectly or to feel that you need to keep up with the Jones'!
Plan your time well. What is really urgent and what is really important? We all enjoy a challenge but be realistic in the goals you set.
Communicate – Ask for what you reasonable need, don't try and be a hero. Think about how you could delegate or ask others for support.
Learn to say 'No' to extra requests or demands, explaining why and when you may be able to do it. Help find a solution.
Nurture a good social network both within and outside work. Help to build a culture of empathy, listening and positivity.


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text:
THE VALENTINE'S DAY COLLECTION
CHEESE SHOP
HANNA'S PANTRY
GRAZING BOXES
GRAZING PLATTERS
CHÂTEAU STE. AGNÈS
VISIT THE VINEYARD
MEET HANNA
La Tur
La Tur is a soft-ripened cheese made from a blend of sheep's, cow's and goat's milk. It is produced by Caseficio dell'Alta Langa in the Alta Lange region of Italy. The cylinder shaped cheese is a light straw yellow colour with an edible soft and wrinkled rind. La Tur tastes of the sweetness of cream and butter, followed by acidic notes and yeasty flavours.
It goes with a wide variety of wine pairings, especially those with floral or honey notes.
Moliterno al Tartufo
Hard or semi hard sheep's milk cheese, the taste of the Moliterno is exalted by the gustative notes of the truffle. The paste is white with a marbling of truffles....
Etorki
The Etorki Basque Cheese has a velvety firm texture with a mild to medium nutty flavour. The basque cheeses are extremely popular because of their subtle, yet flavourful profiles. Etorki is...
Mimolette Extra-Vieille 20 Mois
In French, mi-mou means half soft and refers to the quite oily texture of this otherwise firm cheese. Aged Mimolette is often described as a sharp but mild cheese that...
Le Saint-Just
Full fat soft cheese made with pasteurized cow's milk and pasteurized cream. Ingredients: Pasteurized cow's milk, pasteurized cream, salt, rennet, culture. 180 g
Chabichou
Chabichou is a traditional semi-soft, unpasteurized, natural-rind French goat cheese with a firm and creamy texture. Chabichou is formed in a cylindrical shape which is called a "bonde", per the...
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text:
Q: national characters/unicode characters extract from PDF C# I'm using Tesseract and wrapper - tesseract.net version 4.0.0.16
By using this wrapper i create serchable Pdf.
tessBaseAPI.SetInputName(imagePath);

        using (var pdfRenderer = new PdfRenderer(outputName, tessDataPath, false))
        {
            pdfRenderer.BeginDocument(filename);
            pdfRenderer.AddImage(tessBaseAPI);
            pdfRenderer.EndDocument();
        }

Next I use  PDFsharp-MigraDoc version 1.50.4619-beta4c
to compress PDF and save as stream
Stream pdf = new MemoryStream();
PdfSharp.Pdf.PdfDocument document = PdfSharp.Pdf.IO.PdfReader.Open(filePath);
document.Options.FlateEncodeMode = PdfSharp.Pdf.PdfFlateEncodeMode.BestCompression;
document.Options.UseFlateDecoderForJpegImages = PdfSharp.Pdf.PdfUseFlateDecoderForJpegImages.Automatic;
document.Options.NoCompression = false;
document.Options.CompressContentStreams = true;
document.Save(pdf);

At the end I use iTextSharp version 5.5.13
to extract text from PDF. PDF is read as byte[]
PdfReader reader = new PdfReader(file);
iTextSharp.text.Rectangle rect = new iTextSharp.text.Rectangle(llx,lly,urx,ury);
RenderFilter[] filter = { new RegionTextRenderFilter(rect) };
ITextExtractionStrategy strategy;
StringBuilder sb = new StringBuilder();
strategy = new FilteredTextRenderListener(new LocationTextExtractionStrategy(), filter);
string currentText = PdfTextExtractor.GetTextFromPage(reader, currentpage, strategy);
currentText = Encoding.UTF8.GetString(ASCIIEncoding.Convert(Encoding.Default, Encoding.UTF8, Encoding.Default.GetBytes(currentText)));
sb.Append(currentText);

But my problem is iTexSharp extract text without national characters.
For example:
In PDF is line: "Spółka z ograniczoną odpowiedzialnością - Spółka"
When I open it in Firefox/ Chrome/ AdobeReader next the line is copied as "Spółka z ograniczoną odpowiedzialnością - Spółka"
But in iTextSharp this line is extracted as "SpóBka z ograniczon\u0005 odpowiedzialno[ci\u0005 \u0014 SpóBka"
These are extracted unicode characters:
"ą" = "\u0005"
"-" = "\u0014"
"ę" = "\u0019"
"ć" = "\a"
"ś" = "["
"ł" = "B"
"ó" = "ó"
Do you have any idea where I could change Encoding or Language to make it work properly. I would like to notice that in PDFsharp-MigraDoc I have to open existing file. Also when I skip compression PDFsharp-MigraDoc part, iTextSharp work exactly the same
I can't find any property/option/setting to change encoding.
Do you have any idea how to do it or something else?

redpajama_set_name: RedPajamaStackExchange


Prefab cabins can make your spare time feel like holidays. Many people are thinking of investing in prefab log cabins as hunting cabins.
Or just some safe, quiet place to escape from the rat race of everyday stresses and tensions.
When you are thinking about prefab cabins you can imagine a small, claustrophobic wooden structure build on a wasteland in the middle of nowhere, but you can also think of a beautifully structured cabin on the edge of the woods or near the lake used for a romantic getaway or break.
It is up to you which option you think about, but it is safe to say that most people will go for the second option.
Prefab log cabins can be used for many reasons and can be used intensively or just on rare occasions. Not only can you use them as that romantic getaway we just were thinking about above, but cabin kits can also be used to make a great log cabin base for hunters.
As we always like to think about romance first we look at this option first of course.
Cabin kits are easy to construct and the prefab log cabins do not even need to take up that much space, if you do not want to, so if you own a small piece of land in the woods or near a lake you can use panelized kits to quickly build a cabin for you and your family. Relax with the rustling of the trees in the background or enjoy the fire place whilst listening to some good classic music whilst you are enjoying a good glass of wine.
You can make your prefabricated log cabin as comfy as you want as the inside can be easily decorated in any style you want. This offers the perfect weekend or holiday getaway.
Of course there are also the functional usages of log cabins. The most common other use is the use as a hunting cabin and these prefab hunting cabins are very handy to store your kit for a quick hunting break.
Most hunters will not spend much time in their cabin so functionality is all that is needed. Just a place to sleep well and make a nice dinner before or after the hunt is all that is required. With cabin kits you can go for vey basic structures, or you can give yourself a bit of luxury.
Because of the flexible solutions available when you are looking to purchase cabin kits, you can really make the packages suited to your needs.
If you always wanted to have a little getaway away form other people, than now is the best time to do it. Land can be purchased at an all time low cost and with the prices of prefab cabins also very low you will be able to have the "luxury" of owning a log cabin for a fraction of the usual cost.
This will not only give you more equity, but it will also be a place where you can reduce stress levels, be it because of a quick relaxing break or to release the pressure by stalking and hunting for game.


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

\begin{table*}
\begin{minipage}{\textwidth}
\caption{Fit parameters for the total emission line spectrum at CO(1-0) and CO(3-2).}
\begin{center}
\begin{tabular}{l c c c c c c c c c}
\hline
CO & $\nu_{\rm rest}$ & $\nu_{\rm obs}$ & $\chi^2$/dof & Gaussian & Integrated intensity\footnote{The integrated line intensities have been corrected for the primary beam response.} & Peak & FWHM\footnote{The line widths have been corrected for instrumental broadening.} & Velocity shift & Mass\footnote{The molecular gas mass was calculated from the CO(1-0) integrated intensity as described in section \ref{sec:mass}.} \\
Line & (GHz) & (GHz) & & component & (Jy{\thinspace}km/s) & (mJy) & (km/s) & (km/s) & ($10^{9}M_{\odot}$) \\
\hline
J=1-0 & 115.27 & 102.19 & 100/94 & 1 & $1.5\pm0.2$ & $8.2\pm0.8$ & $170\pm20$ & $-568\pm8$ & $5.0\pm0.7$ \\
 & & & & 2 & $1.7\pm0.3$ & $4.0\pm0.5$ & $400\pm60$ & $-60\pm20$ & $5.7\pm1.0$ \\
J=3-2 & 345.80 & 306.56 & 126/94 & 1 & $5.9\pm0.7$ & $29\pm2$ & $190\pm20$ & $-571\pm7$ & \\
 & & & & 2 & $6.4\pm0.9$ & $19\pm2$ & $320\pm30$ & $20\pm10$ & \\
\hline
\end{tabular}
\end{center}
\label{tab:fits}
\end{minipage}
\end{table*}

Containing molecular gas reservoirs upward of $10^9\hbox{$\rm\thinspace M_{\odot}$}$ and in some
cases approaching $10^{11}\hbox{$\rm\thinspace M_{\odot}$}$, brightest cluster galaxies (BCGs)
are among the most molecular gas rich early-type galaxies in the
nearby universe (\citealt{Donahue00}; \citealt{Edge01,EdgeFrayer03};
\citealt{Salome03}).  BCGs with large quantities of cool gas
reside almost exclusively at the centers of clusters whose hot
atmospheres have short central radiative cooling times ($<1\rm\; Gyr$;
\citealt{Heckman81}; \citealt{Cowie83}; \citealt{Hu85}).  In addition
to molecular gas, these BCGs are forming stars at rates of several to
tens of solar masses per year (eg. \citealt{Johnstone87};
\citealt{ODea08}).  The origin of this gas has been attributed to
either gas rich mergers or cooling from the hot atmospheres
surrounding the BCG.  However, several lines of evidence strongly
suggest that the molecular gas cooled from the hot atmosphere and
accreted onto the BCG fuelling star formation.  Although BCGs harbor
substantial amounts of molecular gas and star formation, this is
typically only a small fraction of the material that is expected to
cool out of the hot atmosphere over time (eg. \citealt{Fabian94};
\citealt{Edge01}; \citealt{Salome03}).

It is now believed that radiative cooling is regulated by
feedback from the active galactic nucleus (AGN;
eg. \citealt{PetersonFabian06}; \citealt{McNamaraNulsen07}).  This so-called
radio-mode feedback is thought to operate primarily on the hot
volume-filling atmosphere, which prevents or regulates the rate of
cooling onto the BCG and in turn the level of fuelling onto the
supermassive black hole (SMBH).  However, the degree to which
radio-mode feedback also operates on the cold molecular gas is
unclear.  Early indications that radio jets interact with the cold
atomic gas have been found in observations of ionized gas in powerful
radio galaxies (eg. \citealt{Tadhunter91}; \citealt{Veilleux02};
\citealt{Emonts05}; \citealt{Nesvadba06}) and HI absorption, which
show high speed outflows of neutral hydrogen
(eg. \citealt{Morganti98}; \citealt{Oosterloo00};
\citealt{Morganti04,Morganti05}).  However, without accurate outflow
mass estimates it is difficult to evaluate their impact on the
evolution of galaxies.

Cycle 0 ALMA observations of the Abell 1835 BCG reveal an apparent
outflow of molecular gas with a mass exceeding $10^{10}\hbox{$\rm\thinspace M_{\odot}$}$.  Its
close association with the X-ray cavities and the
inability of the radiation and mechanical energy from supernovae to
drive such a massive flow of gas suggests that the radio AGN is
powering the outflow (McNamara et al. submitted).  These results imply
that radio mode feedback couples not only to volume-filling hot
atmospheres, but is able to drive outward the high density molecular gas
in galaxies.  Here we present new ALMA Early Science observations of
the BCG in Abell 1664 and report the discovery of massive flows of
molecular gas in the BCG.  We assume $H_0=70\hbox{$\kmps\Mpc^{-1}\,$}$, $\Omega_m=0.3$
and $\Omega_\Lambda=0.7$.  For this cosmology, $1\rm\; arcsec$ corresponds to
a physical scale of $2.3\rm\; kpc$ at the redshift $z=0.128$ of the BCG
(\citealt{Allen92}; \citealt{Pimbblet06}).  This redshift is based
predominantly on emission line observations and is accurate to roughly
$100\hbox{$\km\s^{-1}\,$}$.  All errors are $1\sigma$ unless otherwise noted.

\section{Data reduction}

The BCG in Abell 1664 was observed with the band 3 and the band 7
receivers on ALMA as a Cycle 0 Early Science program (ID =
2011.0.00374.S; PI McNamara).  These data were obtained in two 25 min
observations in band 3 on March 27th and April 7th 2012 and in two 35
min observations in band 7 on March 28th 2012.  On average sixteen 12m
antennas were used in the extended configuration with baselines
out to $400\rm\; m$.  The observations used a single pointing
centred on the brightest cluster galaxy in Abell 1664.  The receiver
was tuned to cover the redshifted $^{12}$CO(1-0) line at $102.2\rm\; GHz$ in the
band 3 upper sideband and the $^{12}$CO(3-2) line at $306.7\rm\; GHz$ in the band
7 upper sideband.  Each spectral window had a bandwidth of $1.875\rm\; GHz$
and two spectral windows were set in each sideband providing a total
frequency range of $\sim{7}\rm\; GHz$.  A spectral resolution of
$0.488\rm\; MHz$ per channel was used but channels were binned together to
improve the S/N ratio.  The bright
quasar 3C\,279 was observed for bandpass calibration and observations
of Mars provided absolute flux calibration.  Observations switched
from Abell 1664 to the nearby phase calibrator J1246-257 every
$\sim10$ minutes.

The observations were calibrated using the \textsc{casa} software
(version 3.3; \citealt{McMullin07}) following the detailed processing
scripts provided by the ALMA science support team.  The
continuum-subtracted images were reconstructed using the \textsc{casa}
task \textsc{clean} assuming Briggs weighting with a robustness
parameter of 0.5 and with a simple polygon mask applied to each
channel.  This provided a synthesized beam of
$1.4\arcsec\times1.1\arcsec$ with PA $-79.1^{\circ}$ at CO(1-0) and
$0.55\arcsec\times0.39\arcsec$ with PA $-81.4^{\circ}$ at CO(3-2).
The rms noise in the line free channels was $0.5\rm\; mJy$ for $40\hbox{$\km\s^{-1}\,$}$
channels at CO(1-0) and $1.5\rm\; mJy$ for $30\hbox{$\km\s^{-1}\,$}$ channels at CO(3-2).
Images of the continuum emission were also produced with
\textsc{clean} by averaging channels free of any line emission.  A
central continuum source is detected in both bands, possibly partially
resolved in band 7, with flux $2.5\pm0.2\rm\; mJy$ in band 3 and
$1.1\pm0.1\rm\; mJy$ in band 7.  The mm-continuum source position coincides
with the VLA radio nucleus position (Hogan et al. in prep).  The
mm-continuum flux is also consistent, within a factor of 2, with
synchrotron emission from a flat spectrum radio core\footnote{For the
  convention $f_{\nu} \propto \nu^{-\alpha}$} with $\alpha\propto0.5$
(Hogan et al. in prep) suggesting this is the location of the low
luminosity AGN.

\section{Results}

\subsection{Spectra and integrated intensity maps}
\label{sec:specinmaps}

We detected and imaged both CO(1-0) and CO(3-2) rotational transition
lines in the BCG of Abell 1664.  Fig. \ref{fig:A1664spectra} shows the
continuum-subtracted total spectral line profiles extracted from a
$6\times6\rm\; arcsec$ region at CO(1-0) and a $3\times3\rm\; arcsec$ region at
CO(3-2).  A larger $6\times6\rm\; arcsec$ region at CO(3-2) produces a consistent total flux but a significantly noisier spectrum.  Both the CO(1-0) and CO(3-2) line profiles show two distinct
components: a broad component centred on the BCG's systemic velocity and
a narrower high velocity system (HVS) blueshifted to $-570\hbox{$\km\s^{-1}\,$}$.
These spectral profiles were each fitted with two Gaussian components using the package \textsc{mpfit} (\citealt{Markwardt09}) and the best fit
results are shown in Table \ref{tab:fits}.  Although the BCG's systemic
component is significantly broader,
the peak flux for the HVS is
roughly a factor of two higher producing a similar integrated intensity for
each component.  The total CO(1-0) integrated intensity of
$3.2\pm0.4\hbox{$\Jy\km\s^{-1}\,$}$ is roughly half of the IRAM single-dish signal
found by \citet{Edge01}.  This may be due to uncertainties in the continuum baseline subtraction, or indicate more extended emission filtered out by the interferometer or lying below our sensitivity.

Integrated intensity maps of the CO(1-0) and CO(3-2) emission are
displayed in Figs. \ref{fig:CO10grid} and \ref{fig:CO32grid}.  This
combination gives a higher resolution image of the molecular gas near
the nucleus at CO(3-2) and sensitivity over more extended scales at
CO(1-0).  The bulk of the molecular gas is concentrated in the galaxy
center within $\sim3\rm\; arcsec$ radius at CO(1-0) and $\sim1.5\rm\; arcsec$ radius
at CO(3-2).  We have produced contours from integrated intensity maps
covering the velocity range of the BCG's systemic component (red) and
the HVS (blue and green) to show their spatial extent.  Both maps show
a similar morphology with these two components separated spatially as
well as spectrally.  The kinematics of these two components broadly
match those found in H$\alpha$, Pa$\alpha$ and ro-vibrational H$_2$
IFU observations of the BCG (\citealt{Wilman06,Wilman09}).

\begin{figure}
\centering
\includegraphics[width=0.98\columnwidth]{A1664CO10CO32_totalspectrumw3vbands.eps}
\caption{Abell 1664 CO(1-0) (top) and CO(3-2) (bottom) total spectra for $6\times6\rm\; arcsec$ and $3\times3\rm\; arcsec$ regions, respectively.  A larger $6\times6\rm\; arcsec$ region at CO(3-2) produces a consistent total flux but a significantly noisier spectrum.  Two component model fits shown by solid line with individual gaussians shown by dashed and dotted lines.  The colored velocity bands correspond to the velocity ranges of the image contours in Figs. \ref{fig:CO10grid} and \ref{fig:CO32grid}.}
\label{fig:A1664spectra}
\end{figure}

In CO(1-0), the BCG's systemic component extends $\sim5\rm\; arcsec$ ($11\rm\; kpc$)
from NE to SW, covering a velocity range from $-250\hbox{$\km\s^{-1}\,$}$ to
$+250\hbox{$\km\s^{-1}\,$}$ and roughly peaking on the continuum position.  The line
emission from this component is highly asymmetric about the nucleus
with the greatest extent towards the NE.  There is approximately twice
as much CO(1-0) flux to the NE of the nucleus compared to the SW.

The HVS extends $\sim4\rm\; arcsec$ ($9\rm\; kpc$) from NW to SE and covers a
velocity range from $-700$ to $-450\hbox{$\km\s^{-1}\,$}$.  It appears marginally to
the N and E of the nucleus and, given the uncertainty in its position
along the line of sight through the galaxy, it is not clear if the HVS
physically interacts with the BCG's systemic component.

The CO(3-2) map shows a broadly similar morphology to the CO(1-0) but
reveals more complex structure on smaller scales.  There is an
apparent drop in the intensity of the BCG's systemic component where it
overlaps with the HVS, possibly suggesting a physical interaction
between these components.  The SW blob of the BCG's systemic component
is roughly spatially coincident with the AGN.  The HVS may separate
into two gas blobs each contained within a projected diameter of $\sim2\rm\; kpc$.
One clump is projected immediately to the N of the nucleus, where the
deficit of emission is seen in the BCG's systemic component.  The second
HV clump appears $\sim3\rm\; kpc$ in projection to the SE and extends toward the N clump.  It could be one extended filament.

\begin{figure}
\centering
\includegraphics[width=0.95\columnwidth]{A1664CO10_momentn720to280kmps_3velcontours_wcrosswlabelslthickwpvline.eps}
\caption{Abell 1664 CO(1-0) integrated intensity map for velocities $-740$ to $300\hbox{$\km\s^{-1}\,$}$ with contours for the disk component ($-300$ to $300\hbox{$\km\s^{-1}\,$}$, red) and the high velocity system ($-740$ to $-540\hbox{$\km\s^{-1}\,$}$, blue, and $-540$ to $-340\hbox{$\km\s^{-1}\,$}$, green).  The contours are -2$\sigma$, 2$\sigma$, 3$\sigma$, 4$\sigma$ and 5$\sigma$, where $\sigma=0.084\hbox{$\Jy{\rm /beam}.{\rm km}\s^{-1}\,$}$ (red), $0.047\hbox{$\Jy{\rm /beam}.{\rm km}\s^{-1}\,$}$ (blue) and $0.046\hbox{$\Jy{\rm /beam}.{\rm km}\s^{-1}\,$}$ (green).  The continuum nucleus is marked by a cross and the ALMA beam size is shown lower left.  The black line shows the axis of the position-velocity diagram in Fig. \ref{fig:A1664pv}.  The image has not been corrected for the primary beam.}
\label{fig:CO10grid}
\end{figure}

\begin{figure}
\centering
\includegraphics[width=0.95\columnwidth]{A1664CO32_momentsn720to270kmps_wcontourswcrosslthickwpvlines.eps}
\caption{Abell 1664 CO(3-2) integrated intensity map for velocities $-735$ to $285\hbox{$\km\s^{-1}\,$}$ with contours for the disk component ($-285$ to $285\hbox{$\km\s^{-1}\,$}$, red) and the high velocity system ($-735$ to $-525\hbox{$\km\s^{-1}\,$}$, blue, and $-525$ to $-345\hbox{$\km\s^{-1}\,$}$, green).  The contours are -2$\sigma$, 2$\sigma$, 3$\sigma$, 4$\sigma$ and 5$\sigma$, where $\sigma=0.25\hbox{$\Jy{\rm /beam}.{\rm km}\s^{-1}\,$}$ (red), $0.15\hbox{$\Jy{\rm /beam}.{\rm km}\s^{-1}\,$}$ (blue) and $0.13\hbox{$\Jy{\rm /beam}.{\rm km}\s^{-1}\,$}$ (green).  Negative contours are shown by a dashed line.  The continuum nucleus is marked by a cross and the ALMA beam size is shown lower left.  The black lines show the axes of the position-velocity diagrams in Figs. \ref{fig:A1664pv} and \ref{fig:A1664CO32pvhighv}.  The image has not been corrected for the primary beam.
\label{fig:CO32grid}
\end{figure}

In Figs. \ref{fig:CO10grid} and \ref{fig:CO32grid}, the HVS has been
sub-divided into higher (blue) and lower (green) velocity contours to
show that the lower velocity gas in this component tends to lie at
larger distances from the nucleus.  There is a shift in the velocity
of the gas in the HVS at CO(3-2) from $-510\pm20\hbox{$\km\s^{-1}\,$}$ in the SE blob
to $-590\pm10\hbox{$\km\s^{-1}\,$}$ in the N clump.  The FWHM of the HVS at CO(3-2) is
$\sim230\pm30\hbox{$\km\s^{-1}\,$}$ in the SE blob but drops to $130\pm10\hbox{$\km\s^{-1}\,$}$ in the
clump to the N of the nucleus.  Although the separate clumps of the
HVS are spatially unresolved at CO(1-0), there is a shift in the
velocity from $-545\pm9\hbox{$\km\s^{-1}\,$}$ to $-600\pm10\hbox{$\km\s^{-1}\,$}$ along the HVS
filament towards the nucleus and a corresponding decrease in the FWHM
from $200\pm20\hbox{$\km\s^{-1}\,$}$ to $130\pm30\hbox{$\km\s^{-1}\,$}$, consistent with the CO(3-2)
results.

The gas clumps labelled A and B in Fig. \ref{fig:CO10grid} appear to
be separate structures with velocities of $-400\pm20\hbox{$\km\s^{-1}\,$}$ and
$-370\pm40\hbox{$\km\s^{-1}\,$}$, respectively.  Using a single Gaussian component
fitted to each spectrum, the integrated intensity was
$0.17\pm0.07\hbox{$\Jy\km\s^{-1}\,$}$ for gas clump A and $0.3\pm0.1\hbox{$\Jy\km\s^{-1}\,$}$ for gas
clump B.  Gas clump A is also observed at CO(3-2) with
an integrated intensity of $0.8\pm0.2\hbox{$\Jy\km\s^{-1}\,$}$ but gas clump B is not
detected.

\subsection{Position-velocity diagrams}

\begin{figure*}
\begin{minipage}{\textwidth}
\centering
\includegraphics[width=0.48\columnwidth]{A1664CO10_pvdiagram.eps}
\includegraphics[width=0.48\columnwidth]{A1664CO32_diskpvdiagrampa13.1.eps}
\caption{Position-velocity diagrams for the BCG's systemic component at CO(1-0) (left) and CO(3-2) (right) each taken through a slice with position angle $77^{\circ}$.  The molecular gas in this structure extends from NE, at velocities of $-250\hbox{$\km\s^{-1}\,$}$, to SW, at velocities of $+250\hbox{$\km\s^{-1}\,$}$.  The contours are -2$\sigma$, 2$\sigma$, 3$\sigma$, 4$\sigma$ and 5$\sigma$.  Negative contours are shown by a dashed line.  The dotted straight line marks the continuum point source position.  The dashed straight line illustrates solid body rotation with $v{\propto}r$.}
\label{fig:A1664pv}
\end{minipage}
\end{figure*}

\begin{figure}
\centering
\includegraphics[width=0.98\columnwidth]{A1664CO32_highvfilpvdiagrampa330.eps}
\caption{Abell 1664 CO(3-2) position-velocity diagram for the HVS taken through a slice with position angle $120^{\circ}$.  The slice runs from SE to NW and is centred on the point where the HVS intersects the BCG's systemic component (see Fig. \ref{fig:CO32grid}).  The contours are -2$\sigma$, 2$\sigma$, 3$\sigma$, 4$\sigma$ and 5$\sigma$.  Negative contours are shown by a dashed line.}
\label{fig:A1664CO32pvhighv}
\end{figure}

Fig. \ref{fig:A1664pv} shows the position-velocity (PV) cuts along a
position angle $\rm{PA}=77^{\circ}$ (defined E from N) across the
BCG's systemic component from NE to SW at CO(1-0) and CO(3-2).  A
two-dimensional Gaussian was fitted to the integrated intensity maps
of the BCG systemic component to determine this best fit PA and this
was found to be consistent at both CO(1-0) and CO(3-2) within the
error.  The PV slices summed the line emission across the width of the
BCG's systemic component.  The CO(1-0) PV diagram shows a smooth
velocity gradient from $-250\hbox{$\km\s^{-1}\,$}$ to $+250\hbox{$\km\s^{-1}\,$}$, with no visible
flattening of the gradient at large radii.  The CO(3-2) emission also
traces this steady velocity gradient.  This appears consistent with
solid body rotation in the rest frame of the BCG implying a constant
mass density core over a scale of $\sim10\rm\; kpc$.  The velocity structure is similar to that of the rotating gas disk in Hydra A (eg. \citealt{Simkin79}; \citealt{Ekers83}; \citealt{Wilman05}; Hamer et al. submitted).  The AGN appears
offset from the gas dynamical center by $\sim0.5\rm\; arcsec$ but this may
instead be due to the uncertainty in the systemic velocity.  The
emission is clumpy and strongly asymmetric about the nucleus at both
CO(1-0) and CO(3-2) suggesting the disk may be only partially filled.

Fig. \ref{fig:A1664CO32pvhighv} shows a PV slice along the HVS from SE
to NW with best fit position angle $\rm{PA}=120^{\circ}$ at CO(3-2).
The HVS may separate into two gas blobs each with a very broad
velocity dispersion of close to $300\hbox{$\km\s^{-1}\,$}$.  The velocity at the peak
intensity shifts from $\sim-450\hbox{$\km\s^{-1}\,$}$ to $\sim-600\hbox{$\km\s^{-1}\,$}$ from the SE
to NW blob but there is not a clear velocity gradient for the intervening gas as found for the
BCG's systemic component.  The PV diagram for the HVS at CO(1-0) shows a
similar velocity structure but at lower spatial resolution.

\section{Discussion}

Our CO(1-0) and CO(3-2) observations show that the BCG in Abell 1664
harbors two large gas flows projected across the galaxy center at
velocities from $-700$ to $-450\hbox{$\km\s^{-1}\,$}$ and $-250$ to $+250\hbox{$\km\s^{-1}\,$}$.
These molecular gas structures and their kinematics match those found
in IFU observations of the BCG covering H$\alpha$, Pa$\alpha$ and
ro-vibrational H$_2$ (\citealt{Wilman06,Wilman09}).  In the following
we calculate the molecular gas masses of these flows and consider
their possible origins including mergers, inflow settling into a disk
and outflow.

\subsection{Molecular gas mass}
\label{sec:mass}

From the integrated CO(1-0) intensities, $S_{\rm CO}\Delta v$, in Table \ref{tab:fits}, we calculated the molecular gas mass

\begin{equation}
M_{\rm mol} = 1.05\times 10^4 X_{\rm CO}\left(\frac{1}{1+z}\right) \left (\frac{S_{\rm CO}\Delta v}{\hbox{$\Jy\km\s^{-1}\,$}}\right) \left(\frac{D_{\rm L}}{{\rm Mpc}}\right)^2\hbox{$\rm\thinspace M_{\odot}$},
\end{equation}

\noindent where $\rm X_{CO}$ is the CO to H$_2$ conversion factor
($\hbox{$\psqcm(\K\kmps)^{-1}$}$), $D_{\rm L}$ is the luminosity distance and $z$ is the BCG
redshift (eg. \citealt{Bolatto13}).  Under the assumption of the
Galactic value $\rm X_{CO}=2\times 10^{20}\hbox{$\psqcm(\K\kmps)^{-1}$}$, we find a molecular
gas mass for the BCG's systemic component of $M_{\rm disk} =
(5.7\pm1.0)\times 10^9\hbox{$\rm\thinspace M_{\odot}$}$ and a mass for the high velocity system
of $M_{\rm HVS} = (5.0\pm0.7)\times 10^9\hbox{$\rm\thinspace M_{\odot}$}$.  The total CO mass in
the BCG is then $(1.1\pm0.1)\times 10^{10}\hbox{$\rm\thinspace M_{\odot}$}$.  The two separate gas clumps, A and B (Fig. \ref{fig:CO10grid}),  have molecular gas masses of $(6\pm2)\times10^{8}\hbox{$\rm\thinspace M_{\odot}$}$ and $(1.0\pm0.3)\times10^{9}\hbox{$\rm\thinspace M_{\odot}$}$, respectively.  The true value of $\rm
X_{CO}$ may depend on environmental factors such as the gas phase
metal abundance, temperature, density and dynamics.

The central gas surface density of $\sim200\hbox{$\Msun\pc^{-2}\,$}$ is not unusual for a
star forming disk (eg. \citealt{Bolatto13}).  The star forming regions produce \textit{U}-band continuum emission from which \citet{Kirkpatrick09} determine a star formation rate of $\sim20\hbox{$\Msun\yr^{-1}\,$}$.  There is no bright point source associated with the AGN.  For a radius of
$\sim3\rm\; kpc$, the surface densities of star
formation and molecular gas are ${\rm log}\Sigma_{\rm SFR}=-0.2\hbox{$\Msunpyr\kpc^{-2}\,$}$
and ${\rm log}\mu_{\rm CO}=2.3\hbox{$\Msun\pc^{-2}\,$}$,
respectively.  The Abell 1664 BCG lies with circumnuclear starbursts
and central regions of normal disks on the Schmidt-Kennicutt relation
(\citealt{Kennicutt98}) showing that despite the massive gas flows it
is similar to other normal galaxies.  The surrounding X-ray
atmosphere, from which the molecular gas presumably cooled, also has a
subsolar metallicity ($0.5-1\hbox{$\thinspace \mathrm{Z}_{\odot}$}$, \citealt{Kirkpatrick09}).
Therefore, we argue that the Galactic $\rm X_{CO}$ value is likely to
be reasonable.  Even if $\rm X_{CO}$ lies a factor of a few below the
Galactic value, the molecular gas flows reported here would still
exceed $10^{9}\hbox{$\rm\thinspace M_{\odot}$}$, which would not qualitatively alter our
conclusions (eg. McNamara et al. submitted).

\subsection{Mergers}

\citet{Kirkpatrick09} noted that at least four galaxies are projected
against the envelope of the BCG raising the possibility of a merger.
Although no galaxy is observed coincident with the high velocity
system, the central optical morphology is complicated by bright knots
of star formation and dust regions (Fig. \ref{fig:hstabsconts};
\citealt{ODea10}).  It is therefore difficult to rule out a collision
but there are several factors weighing against.  The BCG resides at
the center of a dense cluster atmosphere.  A galaxy plunging into the
center would likely be stripped of most of its gas before it reached
the BCG (eg. \citealt{Vollmer08}; \citealt{Kirkpatrick09};
\citealt{Jablonka13}).  Although molecular gas is more resilient to
ram pressure stripping than atomic gas, the molecular gas masses in
the BCG and the HVS are unusually large and there are few galaxies in
nearby clusters harboring this much gas (eg. \citealt{Combes07};
\citealt{Young11}).  In the context of a merger scenario, the
different velocities of the BCG's systemic component and the HVS may
require two unlikely merger events.  These interactions would
also have to be close to direct hits to the BCG center, which again
would be unlikely (eg. \citealt{Benson05}).

\begin{figure}
\centering
\includegraphics[width=0.48\columnwidth]{A1664hstwithCO32nocontourswboxwlabels.eps}
\includegraphics[width=0.48\columnwidth]{A1664hstwithCO32wallcontours.eps}
\caption{Left: HST WFPC2 F606W optical image of the BCG in Abell 1664.  Right: Zoom in of the HST image with ALMA CO(3-2) contours representing the BCG's systemic component ($-285$ to $285\hbox{$\km\s^{-1}\,$}$, yellow) and high velocity system ($-705$ to $-405\hbox{$\km\s^{-1}\,$}$, cyan).  The ALMA beam size for CO(3-2) is shown to the lower left.}
\label{fig:hstabsconts}
\end{figure}

\subsection{Inflow}

It is more likely that such large quantities of molecular gas
originated in gas cooling from the hot cluster atmosphere
(\citealt{Edge01}; \citealt{Salome03}).  In BCGs, there are clear
associations between the shortest radiative X-ray cooling times, the
strength of optical line emission, CO and H$_2$ emission and star
formation (\citealt{Cowie83}; \citealt{Crawford99}; \citealt{Peres98};
\citealt{Rafferty08}).  The BCG in Abell 1664 is among the brightest
H$\alpha$ emitters in the \citet{Crawford99} ROSAT Brightest Cluster
Sample, the H$\alpha$ emission aligns with the soft X-ray emission
(\citealt{Allen95}) and the X-ray radiative cooling time in the center
is short ($0.4\rm\; Gyr$; \citealt{Kirkpatrick09}).  In the nearby BCG
NGC\,1275, the CO filaments are co-spatial with the coolest X-ray gas
and the outer two filaments have radial velocity gradients with larger
blueshifted velocities at smaller radii (\citealt{Salome06};
\citealt{Lim08}).  The molecular gas kinematics are consistent with
free fall in the gravitational potential of NGC\,1275, as expected if
they originated in cooling from the X-ray atmosphere.

For radial inflow, we expect velocity gradients increasing
towards the nucleus with the largest velocities towards the BCG
center.  This is more or less what is seen.  The extent and velocity
gradients across the HVS gas clumps and the BCG's systemic component can
therefore constrain their dynamics and origin
(Fig. \ref{fig:CO32grid}).  The velocity shear across the gas clumps
in the HVS is $\sim250-300\hbox{$\km\s^{-1}\,$}$ along the line of sight
(Fig. \ref{fig:A1664CO32pvhighv}).  A similar shear in the transverse
direction could have separated the clouds on the observed scale in only $\sim10^7\rm\; yr$.
Therefore, the clumps are of order that age or the clouds are moving
nearly along the line of sight.  In
the latter case, the broad velocity shear could signify a velocity
gradient with high velocity infall onto the nucleus.

The BCG's systemic component has a clear and smooth velocity gradient
with a velocity increase of $\sim500\hbox{$\km\s^{-1}\,$}$ over its $\sim11\rm\; kpc$
length.  The velocity profile of this component is suggestive of
rotation about the BCG center, however the mass and velocity structure
are strongly asymmetric (section \ref{sec:specinmaps}).  For a
putative rotating disk, we estimate the Toomre Q-criterion for disk
stability (\citealt{Toomre64}), $Q=v_{\rm c}v_{\rm T}/\pi Gr\Sigma$,
where the circular velocity $v_{\rm c}\sim200\hbox{$\km\s^{-1}\,$}$, the turbulent
velocity $v_{\rm T}\sim50-100\hbox{$\km\s^{-1}\,$}$, the disk radius $r\sim3\rm\; kpc$ and
the disk surface density $\Sigma\sim200\hbox{$\Msun\pc^{-2}\,$}$.  The Q parameter
is of order one suggesting that it could be unstable and potentially
star forming.  However, Fig. \ref{fig:hstabsconts} does not show
strong star formation associated with the BCG's systemic component.
Star formation could be obscured by dust but the \textit{U}-band star
formation rate, $SFR_{\rm U}\sim20\hbox{$\Msun\yr^{-1}\,$}$ (\citealt{Kirkpatrick09}),
and the infrared star formation rate, $SFR_{\rm IR}=15\hbox{$\Msun\yr^{-1}\,$}$
(\citealt{ODea08}), are comparable, which is inconsistent with buried
star formation.  This could be a recent infall of material that is in
the process of settling into a disk around the nucleus.  Its orbital
time is $\sim9\times10^{7}\rm\; yr$ so a relaxed disk will take at least
several $10^8\rm\; yr$ to form.

An X-ray cooling origin for the gas inflow must explain how molecular
hydrogen can form in this environment.  It is difficult to form
molecular hydrogen rapidly in these systems by a process other than
catalytic reactions on dust grain surfaces (eg. \citealt{Ferland94}).
Hot ions in the X-ray atmosphere will destroy unshielded dust on much
shorter timescales than the radiative cooling time
(eg. \citealt{Draine79}).  Yet, dust does appear to be a ubiquitous
feature of the colder gas phases in these systems
(eg. \citealt{Egami06}; \citealt{Donahue07}; \citealt{Quillen08};
\citealt{Mittal11}).  \citealt{Ferland94} have speculated that dust
may somehow form deep within very cold gas clouds, but ab initio dust
formation by coagulation of atoms is likely to be a slow process, and
difficult in an environment where X-rays can quickly destroy small
clusters of atoms (eg. \citealt{Voit95}).  If dust-rich stellar ejecta
from the BCG and ongoing star formation can be mixed into cooling
X-ray gas before the dust grains are destroyed by sputtering, then
those seed grains may act as sites for further dust nucleation
(\citealt{Voit11}; \citealt{Panagoulia13}).  Dusty gas clouds could be
dragged out from the BCG by buoyantly rising radio bubbles and promote
subsequent molecular formation (see section \ref{sec:agnoutflow};
eg. \citealt{Ferland09}; \citealt{Salome11}).

\subsection{Outflow}

Without additional absorption line observations, it is difficult to
determine whether the gas flows lie in front or behind the BCG along
the line of sight.  Therefore, we cannot distinguish between an inflow
of gas located behind the BCG and an outflow of gas located in front
of the BCG.  Fig. \ref{fig:hstabsconts} shows that the molecular gas
clumps appear coincident with regions of lower optical-UV surface
brightness in the BCG, which could indicate either a physical
reduction in the emission or dust obscuration.  Gas clumps A and B are
associated with bright optical-UV knots.  The complexity of the
structure makes a clear interpretation difficult but it is plausible
that the dusty, molecular gas lies predominantly in front of the BCG
and the blueshifted velocities indicate an outflow.

\subsubsection{Driving an outflow with radiation pressure or supernovae}

Radiation pressure from young stars will drive out the molecular gas
if the radiative force exceeds the gravitational force on the cloud,
$L_{\rm UV}/c > Mg$.  We estimates the gravitational acceleration as
$g=2\sigma^2/R$, where the stellar velocity dispersion for a BCG is
typically $\sim300\hbox{$\km\s^{-1}\,$}$ (eg. \citealt{vonderLinden07}) and the
projected extent of the outflow $R=9\rm\; kpc$.  For an outflow mass
$M=5\times10^9\hbox{$\rm\thinspace M_{\odot}$}$, this requires a luminosity in excess of
$2\times10^{46}\hbox{$\erg\s^{-1}\,$}$.  The FUV continuum emission from young stars
in the Abell 1664 BCG provides $L_{\rm UV} = 1.7\times10^{43}\hbox{$\erg\s^{-1}\,$}$
(\citealt{ODea10}), which is insufficient by three orders of
magnitude.

Mechanical winds driven by supernovae can also power molecular gas
outflows in galaxies (eg. \citealt{Veilleux05}).  Assuming
$10^{51}\rm\; erg$ per Type II supernova and a supernova production rate of
1 per $127\hbox{$\rm\thinspace M_{\odot}$}$ (\citealt{Hernquist03}), the star formation rate in
the Abell 1664 BCG of $SFR\sim20\hbox{$\Msun\yr^{-1}\,$}$ will generate a mechanical
power of $\sim5\times10^{42}\hbox{$\erg\s^{-1}\,$}$.  This falls short of the kinetic
power of the outflow, $E_{\rm KE}/t_{\rm
  out}\sim2\times10^{58}\rm\; erg/2\times10^{7}\rm\; yr=3\times10^{43}\hbox{$\erg\s^{-1}\,$}$,
by a factor of $\sim6$ and assumes that all of the mechanical energy
is coupled to the gas.  Little energy can be radiated.  Mechanical
winds from supernovae are therefore insufficient to accelerate the
molecular gas.

\subsubsection{Driving an outflow with a radio AGN}
\label{sec:agnoutflow}

Using ALMA Cycle 0 observations of the BCG in Abell 1835, McNamara et
al. (submitted) found a massive $>10^{10}\hbox{$\rm\thinspace M_{\odot}$}$ outflow of molecular
gas likely driven by the radio AGN.  Active central radio sources and radio
bubbles inflated by the central AGN are ubiquitous in galaxy clusters
with short central cooling times, such as Abell 1664
(\citealt{Burns90}; \citealt{Birzan04}; \citealt{DunnFabian06}).  The
central radio source in the BCG in Abell 1664 is amorphous and fairly
weak, similar to Abell 1835.  The bulk of the energy from the radio
AGN emerges as mechanical energy, which can be estimated using scaling
relations between the jet mechanical power and the radio synchrotron
power (\citealt{Birzan08}).  Using the $1.4\rm\; GHz$ NVSS and $352\rm\; MHz$
WISH catalog radio fluxes of $36.4\rm\; mJy$ and $352\rm\; mJy$ (\citealt{Condon98}; \citealt{DeBreuck02}), respectively, \citet{Kirkpatrick09} estimated a AGN mechanical power of
$\sim6-8\times10^{43}\hbox{$\erg\s^{-1}\,$}$.  However, this has an order of magnitude
uncertainty.  The outflow velocity of the molecular gas is consistent
with the buoyancy speeds of radio bubbles.  These are typically a
significant fraction of the sound speed in the hot cluster atmosphere
(eg. \citealt{Birzan04}), which is $\sim900\hbox{$\km\s^{-1}\,$}$ at the center of
Abell 1664.  For an outflow age of $2\times10^{7}\rm\; yr$, the energy
required to drive a $5\times10^{9}\hbox{$\rm\thinspace M_{\odot}$}$ molecular gas outflow at a
velocity of $600\hbox{$\km\s^{-1}\,$}$ is roughly 35\% of the AGN mechanical energy.
This is large but plausible given the order of magnitude uncertainty
on the AGN mechanical power.

Although there is no detection of a counterpart redshifted outflow,
the asymmetry may be due to uneven mass-loading or a lopsided radio
jet in the previous outburst.  The molecular gas outflow observed in
Abell 1835 (McNamara et al. submitted) is also asymmetric, with a
higher mass and broader velocity dispersion observed in the redshifted
compared to the blueshifted component.

The putative coupling between the radio outburst and the molecular gas
is also not understood.  Simulations have shown that ram pressure
produced by high Eddington ratio jets is able to couple efficiently to
the interstellar medium and drive some of the gas out
(eg. \citealt{Wagner12}).  However, observations of Abell 1835 suggest
that the molecular gas is being lifted by the updraft in the wake of
the radio bubbles (eg. \citealt{Pope10}; McNamara et al. submitted).
It is difficult to understand how small and dense molecular gas clouds
can be uplifted with entrained hot gas.  This could potentially be
explained if the molecular gas formed in situ from hotter
$\sim0.5-1\rm\; keV$ gas rising in the bubbles' wake
(eg. \citealt{Salome08}; \citealt{Revaz08}; \citealt{Salome11}).  The
radiative cooling time of $0.5-1\rm\; keV$ gas in local pressure
equilibrium is only a few $\times10^7\rm\; yr$, which is comparable to the
rise time of the bubbles and the molecular gas.  The $0.5-1\rm\; keV$ gas
would have a density only a few times larger than the ambient hot
atmosphere but it would be several orders of magnitude less dense than
the molecular gas itself, making it much easier to lift and accelerate
to the speeds observed.  Molecular hydrogen is difficult to form
rapidly in these systems without sufficient dust and, if unshielded, dust will be
quickly sputtered by the hot X-ray gas (eg. \citealt{Draine79};
\citealt{Ferland94}).  Dust could, however, be dragged out from the
galaxy centre by rising bubbles and this may be sufficient for
molecular hydrogen formation in extended outflows
(eg. \citealt{Ferland09}).

\section{Conclusions}

Our ALMA Early Science observations of the molecular gas in the Abell
1664 BCG reveal two massive molecular gas flows each with a mass of
$M_{\rm mol}\sim5\times10^{9}\hbox{$\rm\thinspace M_{\odot}$}$.  The component centred on the BCG
systemic velocity shows a smooth velocity gradient across the BCG
center from $-250$ to $250\hbox{$\km\s^{-1}\,$}$ with velocity proportional to radius.
Although this is suggestive of solidy body rotation about the nucleus, the
mass and velocity structure are highly asymmetric and could
indicate an inflow of gas in the process of forming a relaxed disk.
The high velocity system consists of two gas clumps each $\sim2\rm\; kpc$
across at a velocity of $-570\hbox{$\km\s^{-1}\,$}$ with respect to the systemic
velocity.  Each clump has a velocity dispersion of $\sim250-300\hbox{$\km\s^{-1}\,$}$
and there is an increase in the velocity of the gas towards the
nucleus from $-510\pm20\hbox{$\km\s^{-1}\,$}$ to $-590\pm10\hbox{$\km\s^{-1}\,$}$.  This velocity
gradient could signify a high velocity inflow onto the nucleus with
the broad velocity shear indicating the acceleration is along an axis
close to the line of sight.  However, the high velocity system is also
coincident with regions of low optical-UV surface brightness, which
could trace dust extinction associated with each clump.  The high
velocity gas would then be a massive outflow projected in front of the
BCG and moving toward us along the line of sight.  Based on the energy
requirements, we suggest that this outflow would most likely be driven
by the central AGN.  A merger origin for the high velocity system is
possible but we consider it unlikely.

\section*{Acknowledgements}

HRR and BRM acknowledge generous financial support from the Canadian
Space Agency Space Science Enhancement Program.  RAM and ANV
acknowledge support from the Natural Sciences and Engineering Research
Council of Canada.  ACE acknowledges support from STFC grant
ST/I001573/1.  We thank the ALMA scientific support staff members Adam
Leroy and St\'ephane Leon.  This paper makes use of the following ALMA
data: ADS/JAO.ALMA\#2011.0.00374.S. ALMA is a partnership of ESO
(representing its member states), NSF (USA) and NINS (Japan), together
with NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with the
Republic of Chile. The Joint ALMA Observatory is operated by ESO,
AUI/NRAO and NAOJ.  The National Radio Astronomy Observatory is a
facility of the National Science Foundation operated under cooperative
agreement by Associated Universities, Inc.

\lastpagefootnotes

\bibliographystyle{apj}

redpajama_set_name: RedPajamaArXiv


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Country: Germany, Japan, France, USA
Genre: Action, Thriller, Crime
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Transsiberian
Americans abroad. Roy and Jessie finished a volunteer stint in China. He loves trains, so they go home via the Trans-Siberia Express. There are strains ...
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Genre: Mystery, Drama, Thriller, Crime
Actor: Woody Harrelson, Emily Mortimer, Ben Kingsley, Kate Mara, Eduardo Noriega, Thomas Kretschmann, Etienne Chicot, Mac McDonald, Colin Stinton, Perlis Vaisieta, Mindaugas Papinigis, Mindaugas Capas, Sonata Visockaite, Larisa Kalpokaite, Valentinas Krulikovskis
The Machinist
Trevor Reznik is a machinist in a factory. An extreme case of insomnia has led to him not sleeping in a year, and his body ...
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text:
PLACE OF BIRTH: Bellflower, California, United States
OCCUPATION: self employed
EDUCATION: Subject attended school in both Mexico (Baja California) and California.
AREA(S) OF RESIDENCE OUTSIDE REPRESENTATIVE REGION FOR LONGER THAN SIX MONTHS:
Subject was raised in Mexico but was living in Chino Hills, California, in the United States, at the time of this recording.
OTHER INFLUENCES ON SPEECH: N/A
RECORDED BY: Carlos Saldana (under supervision of David Nevell)
DATE OF RECORDING (DD/MM/YYYY): 11/2005
[Interviewer: Tell me about where you and your parents were born.] Uh, I was born here in the United States of America, but I grew up in, I grew up in Mexico. I studied elementary school here and in Mexico. My father is from Guadalajara, Jalisco; my mother is from Mexicali, Baja California, just right here over the border. [Interviewer: Can you tell me about something you feel strongly about?] Something I am passion about now that you mention is, you know, helping Latinos and Chicanos. I really appreciate the movement, the Chicano Movement; I like that. I think it's very important, especially the youth, that they make that an important issue, that they can go over and help the community and give back to the community that gave them. Even though a lot of times it's not as much as they would, you know, would of liked, but still returning that to back the community I think that that's very important. I appreciate that from the students and also from the people, everybody who considers themselves Chicano and say that. I feel proud to say that also that I consider myself Chicano as well. I think that it would be nice if more Latinos would come together as other ethnic groups ha-, you know, really get together and they make things happen and help each other out and we, we lack sometimes that unity, that solidarity that other groups have and I would like to see that. For ourselves to grow and to get, to, to better ourselves as a community and also as a as a society. [Interviewer: What about Antonio Bandera's (a Spaniard) voice in the movement and in Mexico?] He, when he goes to Mexico to film at least that's what I heard when I was in Mexico that he does a lot for, uh, to help the people there and, you know, he's he seems to like it. He considers himself a second a second citizen of Mexico, and I think the Mexicans appreciate it. I don't know politically how much he really does, but I think it's nice that he says it. He says it openly; it's not, it's not something that he keeps to himself so, even though whether it's good or bad, it looks good and that makes the people feel good also, so that's a good thing.
TRANSCRIBED BY: Paul Meier
SCHOLARLY COMMENTARY: N/A
COMMENTARY BY: N/A
DATE OF COMMENTARY (DD/MM/YYYY): N/A


George Clooney's Hollywood career spans more than three decades, with memorable roles including fighting vampires, playing Batman and drifting through space in "Gravity." But Clooney's other accomplishments, including directing, screenwriting and activism, led to him becoming the latest recipient of the American Film Institute's Life Achievement Award.
Clooney, 57, was honored at a star-studded tribute gala earlier this month at the Dolby Theatre, where he has been a frequent guest because of the Academy Awards, including in 2006 when Clooney won for best supporting actor. TNT will air the tribute on Thursday at 10 p.m. Eastern and Pacific.
When Clooney tried to bring attention to the humanitarian crisis in Sudan in 2012, he was arrested for crossing a police line with his father, a moment he said he's proud of. He was also the U.N. designated Messenger of Peace from 2008 to 2014.


text:
NMSU professor receives award for advancing psychology
"I study all things cognitive, mostly visual search research. Think radiologists looking for tumors or TSA agents scanning for weapons in bags."
NMSU professor receives award for advancing psychology "I study all things cognitive, mostly visual search research. Think radiologists looking for tumors or TSA agents scanning for weapons in bags." Check out this story on lcsun-news.com: http://www.lcsun-news.com/story/news/education/nmsu/2018/02/17/nmsu-professor-receives-award-advancing-psychology/348314002/
Billy Huntsman, For the Sun-News Published 1:03 p.m. MT Feb. 17, 2018
NMSU psychology professor Michael Hout and graduate assistant Arryn Robbins demonstrate how they use an eye-tracker system to conduct experiments that examine eye movements and pupillometry.(Photo: Photo by Darren Phillips)
LAS CRUCES - Michael Hout, an assistant professor of psychology at New Mexico State University, is conducting research focused on what people see, the way they see it and why.
"I'm a vision scientist," Hout said. "I study all things cognitive, mostly visual search research. Think radiologists looking for tumors or TSA agents scanning for weapons in bags, but also people looking for everyday items or search-and-rescue teams on patrol."
Hout, a faculty member in the College of Arts and Sciences and associate director of NMSU's Discovery Scholars program, recently received the 2017 Rising Star award from the Association for Psychological Science, a leading international organization dedicated to advancing scientific psychology across disciplinary and geographic borders. The award is presented to psychological researchers in the early stages of their careers.
"One of the most interesting things about psychology and cognition in particular is that our intuition about how our mind works is almost always wrong," Hout said. "A lot of what we do is related to something called the low prevalence effect, which is the sort of counter intuitive finding that says the things you don't find often are harder to find.
"That's a huge problem for someone like a TSA baggage screener because the things they find really often are probably innocuous like water bottles. But if someone gets through security with a gun, which is unlikely to happen but if the TSA screener misses that, it can potentially be a huge problem."
For Hout's research, the subject pool typically consists of volunteers from NMSU's introductory psychology classes. The computer-based experiments allow subjects to tap on a touch-screen monitor to indicate that they've found something or that they've finished searching. To better understand the volunteer's visual search paths, the group uses a desktop eye tracker, which photographs a subject's eyes every millisecond – a thousand times per second. The state-of-the-art eye tracker provides Hout with information about where people look.
"Our primary resource is the departmental eye tracker," Hout said. "We bring them in the eye-tracking room that is dimly lit and set up in such a way that it is conducive to tracking a person's eye movement. So we sit them in front of the computer. There is a large chin-rest that sits in front of them and between them and the computer is a little device that sits on the table that is effectively a camera and an LED. So our participants sit in the eye tracker and they might be searching through displays looking for real world objects, a variety of different things."
Hout balances his time between researching, teaching and service projects. He is engaged not only in collaborations with his graduate students, but with academics around the United States and abroad. He also serves as a journal reviewer for nearly a dozen different scientific peer-reviewed journals and an associate editor for the journal "Attention, Perception, & Psychophysics." In addition he shares his work with other researchers by creating databases that can be used in experimental psychology and sharing many of his software programs.
"I received the award for doing the things I really enjoy doing," Hout said. "I like teaching but I really am passionate about research, mentoring graduate students, writing papers and proposals to bring in grant money."
Hout previously received the Outstanding Scholarship Creative Activities from NMSU's College of Arts and Sciences in 2015, as well as the Early Career Award for Exceptional Achievements in Scholarly Activity from the 16th-annual University Research Council in spring 2016 and the Donald C. Roush Award for Teaching Excellence in fall 2016.
"NMSU and my department make it extremely easy to do my job. I like being an independent researcher, I like being an independent person," Hout said. "The College of Arts and Sciences and the psychology department have provided me with the resources to do my job and to let me conduct my research. That's helped me to be incredibly productive and if I'm productive, I'm happy. I have to do a lot of other work as well but my primary job is to do research experiments and figure out how the mind works, which I'm naturally curious about. I couldn't imagine a more fun job than that."
For more information on NMSU's Vision Sciences and Memory Laboratory, visit http://michaelhout.com.
Read or Share this story: http://www.lcsun-news.com/story/news/education/nmsu/2018/02/17/nmsu-professor-receives-award-advancing-psychology/348314002/


text:
La inmigración francesa en Argentina fue una de las más numerosas de entre todas las de inmigrantes europeos que llegaron a Argentina entre mediados del siglo XIX y mediados del siglo XX. Aunque muy por debajo de las que son por lejos las dos principales corrientes de inmigración en esa época (españoles e italianos), la inmigración francesa se ubicó cómoda en una segunda categoría junto a otras colectividades que también tenían una apreciable cantidad como las de alemanes, rusos y polacos.

Formó así, una de las comunidades de descendientes de franceses más destacadas del continente y del mundo fuera de Europa. Entre 1857 y 1946, 261.020 franceses emigraron a Argentina. De esta cifra, se estima que sólo 100.000 se radicaron de forma definitiva en el país. Hoy, más de 6 millones de argentinos tienen algún grado de ascendencia francesa (hasta un 17% de la población total).

Mientras los argentinos de ascendencia francesa constituyen un porcentaje sustancial de la población argentina, es menos visible que la de otros orígenes de tamaño similar. Esto se debe al alto grado de asimilación cultural, mezcla con otros inmigrantes europeos, en el caso de los inmigrantes vascos franceses a que tenían un trasfondo cultural distinto al del resto de franceses, y en el caso de zonas como el noroeste y Cuyo a la falta de importantes colonias francesas donde se asentaran los inmigrantes franceses para trabajar en cultivos o ganadería.

Regiones de procedencia

La primera oleada de franceses que llegó al país procedía sobre todo de las regiones meridionales de Aquitania y Mediodía-Pirineos. Se embarcaban en Burdeos rumbo a América. Los vasco-franceses constituían además un grupo numéricamente importante.

Integración y colonización

Si bien la mayoría de los inmigrantes franceses se integraron a la vida urbana en la Ciudad de Buenos Aires y el área metropolitana, así como en las otras grandes urbes del país, hubo también proyectos de colonización agrícola. Los más importantes tuvieron lugar en Pigüé (sudoeste del interior de la Provincia de Buenos Aires) y en Chaco (departamentos Primero de Mayo y Bermejo). También hubo pobladores franceses, junto a alemanes y suizos, en la colonia Esperanza, fundada en 1865 por Aarón Castellanos. Otro grupo de inmigrantes franceses se radicó en Oberá, Misiones.

Ciudad de Buenos Aires

La gran mayoría se establece en los alrededores de Plaza Francia, sector de la ciudad que eventualmente se convertiría en lo que hoy es el conocido barrio de la Recoleta. Desde el 1840, llegan los grandes emprendedores franceses, paisajistas y arquitectos, invitados por el gobierno argentino de la época con el propósito de la creación de parques y modernización del diseño urbano. Los mismos dan lugar a una nueva urbe espejo de París en Latinoamérica. Entre los más renombrados se encuentra el paisajista Carlos Thays y su equipo de expertos parisinos, quienes darían a Buenos Aires su aspecto de ciudad luminaria del neoclasicismo francés.

Provincia de Buenos Aires

Pigüé

La ciudad de Pigüé fue fundada como una colonia francesa en 1884. Sus primeros habitantes eran originarios de la región histórica francesa del Rouergue en Occitania.

Villa Francia

Villa Francia fue fundada en 1909 por el colono Louis Lariguet, y le debe su denominación a la nacionalidad de aquel pionero.

Chaco

Inmigrantes franceses, junto a inmigrantes friulianos (nordeste de Italia) y eslovenos fundaron en 1890 la localidad de Margarita Belén, considerada un ejemplo de cooperativismo en Argentina. La ciudad se encuentra 21 kilómetros al norte de Resistencia, capital provincial.

Corrientes

Bonpland

Una de las colonias francesas más importantes en la provincia de Corrientes es la ciudad de Bonpland.

Mendoza

La colonia francesa de San Rafael se constituyó en un importante destino para inmigrantes franceses asentados en la provincia de Mendoza de la mano de Julio Gerónimo Balloffet.

Tucumán

La inmigración francesa en Tucumán está vinculada no solamente con la transformación de la industria azucarera operada a partir del primer influjo de 1830, sino también a la llegada de mano de obra capacitada, entre ellos panaderos, albañiles, artistas plásticos, técnicos ferroviarios, arquitectos, etc, muchos de ellos arribando también a partir de 1876 con la inauguración de la primera vía férrea (Ferrocarril Mitre) que uniría Tucumán con Buenos Aires. La azucarera es la primera industria pesada de la República Argentina y los ingenios serían operados por los técnicos franceses que enviaban las empresas fabricantes. El hijo de un inmigrantes francés, Luis Federico Nougués, se convertiría en gobernador de la provincia de Tucumán en 1906.

Estos son algunos de los apellidos de inmigrantes franceses a partir de 1830: Nougués, Rougés, Fagalde, Guerineau, Bascary, Apestey, Hileret, Berho, Dubourg, Marteau, Delgare, Etcheverry, Martorelle, Duport, Délaporte, Delacroix, Dode, Dupuy, Durrels, Dubois, Chamboud, Jambeau, Beltrés, Revol, Bugeau, Ardois, Abadie, Barraud, Delmas, Devillers, Bergeire, Elizalde, Etchecopar, Feraud, Gaillac, Haurigot, Lalanne, Lescarret, Merchot, Moulins, Tranchard, Pocous, Cartier, Parron, Soutadet, etc.

Cifras

Hacia el 31 de diciembre de 2014, unos 14.548 ciudadanos franceses estaban inscriptos en los registros consulares en Argentina. Casi el 80 % registró su residencia en el área metropolitana de Buenos Aires. También hay grupos en las provincias de Córdoba, Mendoza y Santa Fe. De los inscriptos, el 85 % nació en Francia.

Sexo y grupos de edad

Según el censo argentino de 2010, del total de 6.995 personas nacidas en Francia, 3.513 son hombres y 3.482 mujeres. Del total de hombres, 322 tienen entre 0 y 14 años, 2.386 entre 15 y 64 y 805 son mayores de 65 años de edad. Del total de mujeres, 302 tienen entre 0 y 14 años, 2.098 entre 15 y 64 y 1.082 son mayores de 65 años.

Distribución territorial

El censo argentino de 2010 registró 6.995 personas nacidas en Francia. La siguiente tabla muestra la distribución en las 24 jurisdicciones de primer orden que conformarn la Argentina (23 provincias y la Ciudad Autónoma de Buenos Aires):

Instituciones notables

 Alianza Francesa

 Hospital Francés

Argentinos de origen o ascendencia francesa notables

Véase también
 Inmigración en Argentina
 Inmigración nórdica en Argentina
 Inmigración croata en Argentina
 Inmigración croata en Chile

Referencias

Enlaces externos

Relaciones Argentina-Francia


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