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New Propaganda and Desinformation Challenges for Visegrad
Online Media Literacy
SlovakAid Program
Pro-Kremlin propaganda in Belarus
Toxic VK groups and pages
Бел/Ру
Propaganda and Disinformation Challenges
Publications|Articles
The financial sector of the Belarusian economy at the times of COVID-19 and economic sanctions
Author: Siarhiej Naurodski
Photo: perspectivecenter.org
Belarusian economy demonstrated one of the best performances among European countries in 2020 as it recorded -0.9% of GDP growth (compare to -6.0% for the EU27). In the first half of 2021 the economy showed 3.3% growth, down from 5.4% in the first quarter of 2021.
Key challenges for the economy
However, the comparatively good results of the Belarusian economy do not seem to be convincing enough in terms of sustainability, while its full recovery is still ahead. The officially forecasted nominal 2021 GDP in US Dollars is expected to be 5% below the 2019 GDP. The political crisis in the country after the presidential elections in August 2020 put a serious threat for the economic prospects due to the most recent EU, US, UK, and Canada economic sanctions, massive migration of employees and businesses, as well as general downturn in business activity as a result of politically motivated business check-overs and closures. Economic sanctions among others include ban on export for key state-owned companies and ban on capital support to Belarusian state-owned banks from Western financial institutions.
The political crisis and sanctions amplify two structural weaknesses of the Belarusian economy that seem to be crucial for a fast recovery in post-COVID world:
— Ensuring the rapid growth of small and medium-sized businesses (SMEs) by providing stable sources and new ways of financing for SMEs. The share of SMEs in 2020 GDP was 26.4% (in fact, unchanged from 26.2% in 2012), while their share in export in 2020 was 42.8% (compare to 48.4% in 2015), and share in total investment in 2020 was 40.1% (42.3% in 2014);
— Expansion of the financial sector and an increase in its size relative to GDP by growing assets of banking sector and creation of new accumulative financial products and intermediaries. In q1, 2021, the financial sector size was 42.7% of GDP, which was less than a year ago (46.1%).
The above challenges indicate that significant financial resources will be needed for the recovery coming from the financial system of Belarus. The main challenge for the financial sector in the country thus will be to ensure increase in lending and general stability of financial institutions despite potential effects of the Western sanctions ever-coming as decreased flows from export and limited capital support from the Western banks. To ensure the stability of banks and financial stability in general, the quality of the prudential policy of the National Bank and its independence in decision-making will play a key role. The Belarusian banking sector will have to channel most of the funds for the economic recovery. Non-banking financial institutions, primarily the Development Bank and leasing companies, will be important financial players in providing investments, including for small and medium-sized businesses and entrepreneurship.
The National Bank of Belarus
Currently, the National Bank of Belarus (NBB) has a tough choice between softer monetary policy for faster recovery and tighter monetary policy to fight growing inflation (9.8% yoy in July 2021). Refinancing rate has been raised to 9.25% in July 2021 (up from 7.75% in July 2020), while in general monetary policy is promised to remain countercyclical at least until the end of 2021.
Ensuring the macrofinancial stability in Belarus seems to be the key goal for the National Bank of Belarus in coming months. Keeping monetary policy countercyclical is a challenge in an authoritarian country, like Belarus, where a central bank is only formally independent. Chasing stability in case of Belarus will require from the NBB combination of both traditional monetary policy tools and special considerations:
Maintaining the capital and liquidity of banks at a level sufficient for the economic growth, but without excessive growth of credit risks. Currently non-performing assets as of NBB definition stand at 5%, but for some of the banks this indicator is above the 10% safe line;
Scrupulous checking financial stability indicators, especially in state-owned banks that are subject to the Western financial sanctions (share of four biggest state-owned banks' assets in 2020 was 73%);
Increasing the volume of reserve assets in foreign currency that are currently 47% of the total NBB reserve assets (figure 1);
Putting further efforts to reduce dollarisation level of the banking system in Belarus (currently 48% loans are nominated in foreign currency).
Figure 1. NBB reserve assets in foreign currency, USD mln. Source: NBB
The banking system
Banks remain the key channel of borrowing in the Belarusian economy, both for the private sector and the state-owned enterprises (SOEs) that are equal in size and each making around half of Belarus' GDP. However, the financial condition of SOEs is the key threat to the financial stability of the banking system in Belarus, and this has not changed since the previous crisis in 2015. The deterioration of financial condition of companies controlled by the state directly influences the level of non-performing assets (NPA) in the banking system. Although in the banking system as a whole NPA indicator is below the critical level of 10%, the share of non-performing assets issued to enterprises in foreign currency among state-owned banks is above banking system's average. Due to an impact coming from ever-increasing volume of the EU, US, UK, and Canada sanctions targeting large state-owned companies in Belarus[1], the risk of deterioration of banking assets remains high.
Vulnerability of Belarus banks' funds is another issue for the country's banking system. Deposits show negative dynamics in 2021. For the first half of 2021, total deposits decreased by 3.8%, while the value of individual foreign currency deposits slumped by 13.4%. The share of foreign currency deposits in the banking system exceeds 50%, with a significant part of these deposits held by individuals, who are more susceptible to panic during the crisis. In this regard, de-dollarasation comes out to be an important direction for the general stability in banking sector in the nearest future.
As sanctions will be evolving their impact in coming months, safe level of liquidity of banks in Belarus will be correlated not only with the prudential policy of the National Bank of Belarus, but also with access of banks to new capital on the open market as well as financial guarantees of the government for anti-crisis credit programs implemented via state-owned banks.
Non-bank financial sector
Non-bank financial institutions will play an important role in the economic recovery in Belarus, primarily due to the greater flexibility of their instruments, as well as due to the widespread availability of products for small and medium-sized businesses, micro-organizations, entrepreneurs and individuals.
The depth level of the non-bank financial sector was 32.5% of the entire financial sector (Figure 2, up from 30.1% in q1 2020) and 14% of GDP in q1, 2021.
Figure 2. Belarus' financial sector structure in q1, 2021 Source: own calculations based on NBB data
In Belarus, a market for so-called quasi-bank financing instruments or shadow banking doesn't exist, therefore, among the available non-bank financial intermediaries, the Development Bank of Belarus (DBB) and leasing companies will become the most demanded for investments. The DBB volume of penetration into the economy is directly related to the volume of anti-crisis governmental programs. The amount of DBB bonds in remaining months of 2021 has been tripled in June 2021, which indicates the high level of desperation of the government to maintain economic growth, but with little details on where this money will be spent and their impact on the general financial stability.
The level of penetration of leasing into the economy (the volume of financing for new businesses) currently stays at a decent level of 2.4% of GDP being an important source of investments for companies and individuals. The role of microfinancial institutions in Belarus remains relatively small (the size of loans issued is 0.3% of the size of the financial sector in 2020). In post-pandemic recovery microfinance will remain an important channel for maintaining liquidity for entrepreneurships and individuals. However, the key precondition for non-bank financial operations growth is whether the general macrofinancial stability will be kept at the times of the Western sanctions later in 2021 and in 2022 if no political dialogue begins.
The article was prepared by a participant of the SlovakAid scholarship program.
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× 25.12.2022
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Andrey Kalikh × 20.12.2022
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Creating a cozy corner to curl up, read a good book, chat with an old friend or simply sit and be mindful is a great way to take care of yourself, feed your own soul and recharge your batteries, so you can bring your best self to your family, to your relationships and to whatever it is that you do…inside or outside of the home.
When budgets are stretched (to buy diapers, help pay for your kids' college or just to save for a rainy day), why not "shop" your own house for ways to create your own little niche? When's the last time you "shopped" your house?
I've longed for a dreamy, cream-colored, tufted chair for this corner for a while now…which may or may not happen. The actual chair I'm using was purchased about 20 years ago, when my second child was just a baby. It's a Lazy Boy wingback recliner that is a brick red, but that's only half the story.
I can clearly remember shopping for this piece of furniture two decades ago. It's the chair on which I kissed tiny toes, brushed away the tears of three kids, visited with family and friends…and dreamed about the future.
It's also a chair which has logged thousands of hours of "consultation" time, as I provided early childhood mental health consultation to Head Start, Early Head Start and similar programs in the Midwest. I still use this chair for this purpose.
When you fill your little restful place with things that tell a story, it's that much more meaningful when you can spend time there.
You can take a peek below at what the chair looked like "before". The chair has held up amazingly well. It is comfortable and has aged quite nicely. I wanted to slipcover it to have it fit with my current decor. It was a toss up between the slipcover or buying that much desired tufted chair. Due to the sentimental value of the chair, I've been wavering. Plus…I like to be frugal when I can…and challenge myself to do so on a regular basis.
The brick red was just wrong for this space…plus, it gobbles up all the light in the room…not a positive when the sun only makes rare appearances throughout the winter in this northern clime.
After "shopping my own house", I came across an afghan my mom had made me about 15 years ago. It has an area that needs repairing, so I had it stowed away for mending. It seemed like it might be a good option and sure enough, it was perfect! Quick, easy and instant way to change the look. Granted, it's not a fitted slipcover (which I also love), but it is functional, it was free and it ties everything together.
That tufted, dreamy chair may one day sit where the ole' Lazy Boy now stands…but THE chair will always have a place of honor in our home.
Maybe you don't have a blanket or cover-up for the furniture you are trying to transform, that matches the decor in the room in which the chair will reside. You still have some cost-effective options to cover your piece.
You can purchase a relatively inexpensive throw to cover the chair or go with a fitted slipcover. We've used SureFit Slipcovers at our house years ago, and they worked quite well when the kids were little.
Additionally, there are plenty of tutorials around the web, on you-tube and multiple other online destinations. A quick Google search, or Pinterest visit will yield big results! I considered trying to cover the chair myself, but thought otherwise after reviewing my options.
Gallery Walls: Keep It Odd!
Putting up a mini-gallery wall…or a larger one? The rule of thumb is to keep your number as an odd number. Interior designers may refer to this as the "Rule of Three", reflecting the fact that three seems to be the magic number to create visually appealing vignettes and arrangements. Really, you can use 1, 3, 5 or 7 and so on. These types of arrangements are just more pleasing to the eye. Try it!
Our vignette above was put up in less than five minutes. Each picture has it's own story, as well. We'll share that on Instagram in a few days.
How do you reuse, repurpose and upcycle things around your house?


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Территориальный парк Кол-Ривер-Спрингс () — парк территории Юкон, Канада, созданный в 1990 году на юго-востоке Юкона на реке Кол. Является первым экологическим охраняемым объектом территории. Создание парка стало плодом объединённых усилий правительства Юкона, общины первых народов Лиард и общественной организации по сохранению природы Канады.

Подземные источники сформировали серию известковых террас с холодной водой. Террасы сформированы из туфа, осадочного известняка, и растут по 2—3 см в год. Основной задачей является сохранение дикой природы парка и хрупких образований туфа.

Из-за микроклимата источников, которые не замерзают зимой, и постоянного течения, в парке встречаются необычные для территории виды растений. Например, здесь растёт голубая трава (Poa ammophilla), ложная сассапарель (Aralia nudicaulis), белоплодный и красноплодный воронец (Actaea rubra), горец живородящий (Polygonum viviparum) и уруть мутовчатая (Myriophyllum verticillatum). Животный мир представлен черными медведями и гризли, стаями волков и бобрами, устраивающими плотины.

Парк расположен в 65 км к востоку от озера Уотсон на границе территории Юкон и провинции Британская Колумбия. В связи с полной изолированностью района и хрупкой природой парка доступ к нему ограничен. Любители водного туризма могут добраться до парка от озера Уотерсон по реке Кол, вниз по течению реки находятся пороги 3-го и 4-го уровня сложности. Есть и пешеходный маршрут до парка, препятствием на котором служит опасная горная река. Остальные могут добраться до парка на вертолёте от озера Уотсон.

Примечания

Появились в 1990 году в Канаде
Территориальные парки Юкона

redpajama_set_name: RedPajamaWikipedia


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High School Tennis
Cold Spring Harbor Crowned Long Island Boys Tennis Champions
| By Gary Simeone
The Cold Spring Harbor Boys Varsity Tennis team won their third consecutive Long Island Championship on Wednesday, May 26, knocking off Suffolk County Boys Tennis Champions Half Hollow Hills East by a score of 6-1 at Smithtown East High School. Battling temperatures in the 90s and high humidity,...Read more
Suffolk County Boys Honored at Varsity Tennis Awards Dinner
| By Joe Arias
The Suffolk County Junior Tennis League (SCJTL) revived the Boys Varsity Tennis Awards Dinner with a resoundingly successful event on May 25. This event had not been held in three seasons, but made a strong comeback this year thanks to the effort of SCJTL staff of Joe Arias, Donna Arias, Jimmy...Read more
Cold Spring Harbor Rolls into the Boys Long Island Championship
First singles player, Josh Levine of Cold Spring Harbor thought he would be getting a little more competition from his match against Roslyn at Garden City High School on Thursday. "I was ready to play Austin (Blau) but they told me he had gotten sick and wouldn't be available. So I ended up playing...Read more
Morris Takes Singles Title as Barry & Rubin Win Doubles Title in Nassau County Championship
This past weekend, the best boys high school players in Nassau County came together at Oceanside High School for the Individual Championships. They were battling for County supremacy, as well as a trip to the State Championships (beginning June 3). The weather cooperated this past weekend, allowing...Read more
Great Neck North Takes Thriller Over Syosset
| By Bobby Colton
It all came down to one, single set: Syosset High School's Stephen Peng against Great Neck North High School's Brandon Thomas. One set to determine who would advance in the playoffs and earn a trip to the semifinals to take on Roslyn. Syosset and Great Neck North split their regular season matchups...Read more
Suffolk County Boys Division I Individual Tennis Championship Results
The Suffolk County Boys Division I Individual Tennis Championships were held yesterday at Sachem East High School. Congratulations to all of the players on another successful season of boy's high school tennis ... Singles Championship Nolan Gelman (1) of Half Hollow Hills West defeated Scott...Read more
Cold Spring Harbor and Syosset Square Off Against Each Other and the Elements
To Cold Spring Harbor and Syosset, the prospect of facing off against the opposing school was overshadowed by the daunting task of beating the brutal wind that ripped through the tarp-less fences surrounding the courts. It was clear before the match that neither club was as prepared for the battle...Read more
Two Time Champions Cold Spring Harbor Takes Down Syosset for Second Win
Apr,22,2010
As the bus for Cold Spring Harbor rolled into Syosset's parking lot on Monday, the entire team was looking forward for another chance to prove themselves as the elite team on long island. Led by eight ranked members, Cold Spring Harbor was ready to stake their claim to an undefeated season. Morale...Read more
Long Island Boys High School Preview
2009 season recap Last year, Cold Spring Harbor was crowned winners of the 2009 Nassau County Championship, while in Suffolk, Commack High School was the winner of the 2009 Suffolk County Championship. Cold Spring Harbor went on to defeat Commack 5-2 in the Long Island Championship to capture the...Read more
2009 High School Boys Recap
Jul,01,2009
Nassau County (Section VIII) Tennis Boys Varsity 2009 Final Records Conference 1 1. Syosset 5-8 2. Jericho 9-5 3. Roslyn 10-4 4. Hewlett 1-13 5. Great Neck South 5-8 6. Great Neck North 3-11 7. Long Beach 9-5 8. Cold Spring Harbor 13-1 Conference 2A 1. Bellmore J.F.K. 4-10 2. Wheatley 12-2 3...Read more


1148 01148 ROSES 9″ JUMBO TOILET TISSUE 2 PLY 12/cs.
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207 207 ROSES ROLL TOWEL BROWN 12/600ft.
210 210 ROSES ROLL TOWEL WHITE 6/800ft.
42196 R42196 ROSES TOILET TISSUE 4.3″ x 3.1″ 2 PLY 96/500sht.
52308 52308-2 ROSES CENTER PULL TOWEL 2 PLY 6/600sht.


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Home | Services | Find a consultant
Service A to Z
Our hospitals
How to refer (GPs)
How to refer (patients)
Prof Alastair Sutcliffe
Email: alastair.sutcliffe@nhs.net
University College Hospital
Children and young people's general services, Children and young people's services
Alastair Sutcliffe is a specialist in both general and adolescent paediatrics. He is a Reader in Child Health at the General and Adolescent Unit, of the Institute of Child Health, UCL and his NHS appointment is Hon Consultant Paediatrician.Alastair trained in Manchester but moved to the National Children's Hospital in 1995 and was subsequently appointed a consultant at the Royal Free Hospital (2001-6). He joined UCLH in 2006. He has an MD from UCL and a PhD from the University of Brussels surrounding his work studying children born after IVF for which he is an internationally known authority. Clinically he is interested in general paediatics , runs the secondary epilepsy clinic and is also involved with clinical therapeutics. Alastair has a number of national roles, including being academic convenor for the RCPCH general paediatics group, Chair of the CSG in general paediatrics and Associate Editor for the Journal Human Reproduction. Alastair is a principle contributor to the BNF for Children and Associate Director of London South East LRN.
Dr Sutcliffe's research group presently are working on 10 projects 7 of which have peer reviewed funding from Cancer Research UK, Wellcome Trust, NIHR, and the EU.Projects include ongoign studies of IVF children (cancer risk, epigenetics) their Mothers (Cancer risk) A study of Older Mothers and their offspring, a study of tongue tie treaments (randomised controlled trial) and a number of other projects.
Over 100 Peer Reviewed Papers.
GMC/GDC number: 3190281


Thank you so much for sharing both your support and concerns about the I Trust Women project. It is not my desire in any way to be a force of division in the world, it is very much the opposite…and quite honestly, I have no intention of Kindnessgirl becoming a platform for politics in the future. It really just isn't my thing.
I just know I try to follow my heart everyday…and this particular day, it was loud and I'm not really sure why it was so loud, but it was. I thought about it long and hard as I knew it may even hurt some of you and I would risk losing your presence in this beautiful space. This is a scary place for me to be because I care so deeply, about each of you, and your thoughts and feelings. And in some ways, I still have mixed feelings on the subject too. Yet I am grateful to have a space where I can write, be all of myself and follow my heart, wherever that may be.
I hope we can agree to honor our differences and come back together on new projects that call to each of us, because I believe there will be so many more.
The I Trust Women project will go from now until 2/29.


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CDC director says face masks "more guaranteed" to protect against coronavirus than any vaccine
Friday, September 18, 2020 by: Ramon Tomey
Tags: Anthony Fauci, badhealth, badmedicine, CDC, China Virus, coronavirus, covid-19, face masks, infections, masks, novel coronavirus, outbreak, pandemic, Public Health, Robert Redfield, SARS-CoV-2, vaccination, vaccines, WHO, Wuhan coronavirus
(Natural News) Dr. Robert Redfield, director of the Centers for Disease Control and Prevention (CDC), said in a Sep. 16 Senate hearing that using face masks is "more guaranteed" to protect against the coronavirus than getting the COVID-19 vaccine. Redfield exhorted Americans during the hearing to not dismiss the effectiveness of wearing a mask.
Redfield responded to questions on how the Trump administration responded to the pandemic during the Sep. 16 hearing of the Senate Appropriations subcommittee. The inquiry touched on the subjects of testing, vaccine development and case counts. Dr. Redfield also stressed the importance of mask-wearing, as a potential vaccine being developed might not work for everyone with its 70 percent efficacy rate.
He added that in case the vaccine fails to build an immune response to the coronavirus, the face mask will still safeguard against future infection.
Assistant Secretary of Health Adm. Brett Giroir seconded Dr. Redfield's explanation, telling lawmakers that wearing a mask or face covering "is one of the more important things we can do" to stop the spread of the coronavirus. People who are infected yet do not show symptoms could still be spreading the virus, Adm. Giroir added.
Both the CDC and the World Health Organization (WHO) now suggest that people wear face masks covering both the mouth and nose in order to block respiratory droplets produced when a person coughs, sneezes or talks – especially when people cannot maintain the six-foot distance from others. (Related: Study shows mask-wearers more likely to disregard social distancing guidelines.)
Face masks vs. vaccines
According to a July 2020 study published in the American Journal of Preventive Medicine, a COVID-19 vaccine should have at least 60 percent efficacy to extinguish the current pandemic, assuming that 100 percent of the population is vaccinated. Furthermore, a COVID-19 vaccine would have to be 75 percent effective if only 75 percent of the population gets vaccinated.
Editor's note: Given the rushed research and skipped trials, any coronavirus vaccine is extremely unlikely to show efficacy beyond about 10 percent.
Some medical experts such as Dr. David Heymann, who led the WHO's response to the Severe Acute Respiratory Syndrome (SARS) epidemic, have expressed skepticism toward efforts to fast-track a vaccine. Speaking to The Guardian in May 2020, Heymann doubted if a vaccine can even produce an immune response that would protect against future infections.
National Institute of Allergy and Infectious Diseases (NIAID) head Dr. Anthony Fauci said in August that scientists are hoping to create a vaccine that's at least 75 percent effective – as there was a slim likelihood of creating a COVID-19 vaccine providing 98 percent protection or more.
The U.S. Food and Drug Administration (FDA) has said it would authorize a coronavirus vaccine if it is safe and at least 50 percent effective.
When questioned about the amount of vaccine doses ready, Redfield answered that there are limited quantities available and that those who needed vaccination the most – such as healthcare workers – will get the first doses. He gave an estimate of about "six to nine months" before the entire public gets vaccinated.
Redfield echoed the need for an effective vaccine before Americans could go back to their normal lives in a statement emailed to CNBC. However, he said that "the best defense we currently have … are wearing a mask, washing your hands, social distancing and being careful about crowds" given that there is no approved vaccine yet for COVID-19.
While the CDC and WHO suggest wearing masks, it should ideally be not mandatory. However, some U.S. states are making mask-wearing compulsory – with people being arrested for noncompliance.
The U.S. has the highest COVID-19 caseload as of writing with over 6.6 million cases, 196,804 deaths and 2.5 million recoveries.
Find out more information about how the U.S. and other countries are responding to the Wuhan coronavirus pandemic at Pandemic.news.
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Next : AG Barr: Coronavirus lockdowns "greatest intrusion on civil liberties" since slavery
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https://www.naturalnews.com/2020-09-18-face-masks-protect-against-coronavirus-more-than-vaccine.html
CDC director says face masks "more guaranteed" to protect against coronavirus than any vaccine


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« OC Political Advertisement: Landslide Communications Slate Mail
North Orange County Community College Officials received hidden gifts »
55th AD Watch: Popular Assemblyman Curt Hagman endorse Phillip Chen
Posted by Allen Wilson on October 29, 2013
OC Political just received this press release from Phillip Chen Campaign for Assembly in the 55th AD (Brea, Diamond Bar, Yorba Linda):
Assemblyman Curt Hagman Endorses Phillip Chen in AD 55
YORBA LINDA, CA – – Republican State Assemblyman Curt Hagman has endorsed Phillip Chen as the next Assemblyman in the 55th district, which Hagman currently represents. The highly coveted endorsement from the popular incumbent Curt Hagman solidifies Chen as the clear frontrunner in the June election.
"I am endorsing Phillip Chen to continue my work representing the people of the 55th district. Phillip's background as a reserve deputy sheriff, School Board Trustee and small business owner gives him important insight on the most important issues facing our area – jobs, education and crime. I am extremely confident that Phillip Chen will be an outstanding new conservative member of the Assembly for our district," stated Hagman who has represented the Orange County, Los Angeles and San Bernardino based district since 2008.
"I am very honored to receive Assemblyman Curt Hagman's endorsement and I look forward to continuing the standard he has set with his strong, conservative leadership," said Chen.
Phillip Chen is a small business owner and USC Professor who was the top vote-getter in the Walnut Valley Unified School District Board election in November of 2011. He is a top advisor on health care issues to Supervisor Mike Antonovich and a reserve Deputy Sheriff for the L.A. County Sheriff's Department. Phillip was appointed by Governor Pete Wilson to serve in the Governor's Office of Criminal Justice Planning, where he worked on legislation involving foster care, gang prevention, drug awareness, and mental health.
Phillip is a Doctoral Candidate at USC, he has a Master's in Public Administration from USC and holds a B.A. in Communications from Cal State Fullerton. In addition, Phillip teaches Public Administration as an Adjunct Professor at USC.
This entry was posted on October 29, 2013 at 4:47 PM and is filed under 55th Assembly District, Brea, California, La Habra, Placentia, State Assembly, Yorba Linda. Tagged: 55th Assembly District, Curt Hagman, Phillip Chen. You can follow any responses to this entry through the RSS 2.0 feed. You can leave a response, or trackback from your own site.
One Response to "55th AD Watch: Popular Assemblyman Curt Hagman endorse Phillip Chen"
It is obvious that Phillip Chen will whoop all candidates in the Republican primary. After all, you have someone working as a voluntary sheriff, deputy to Supervisor Anotonvich, and also works as an adjunct Professor. So this will be an automatic win for sure.


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\section{Introduction}
\label{intro}

High-mass stars are known to usually form as multiple objects in the
center of dense clusters (e.g., \citealt{zinnecker2007}). With their
large energy output throughout their whole lifetime and their
clustered nature, they are among the most important ingredients of the
Milky Way and extragalactic systems. However, their actual formation
processes are still not well constrained (e.g.,
\citealt{mckee2007,beuther2006b,zinnecker2007}). Particularly
important questions relate to the fragmentation of the innermost dense
cores and the formation of massive accretion disks (e.g.,
\citealt{krumholz2006b,krumholz2009,beuther2007d,bontemps2010,peters2010b,commercon2011,kuiper2011,kuiper2012}).
While Keplerian accretion disks have been found from low- to
intermediate-mass star-forming regions (e.g.,
\citealt{simon2000,schreyer2002,cesaroni2005}), high-mass star-forming
regions have so far usually exhibited non-Keplerian rotation
signatures on scales between a few 1000\,AU and 0.1\,pc (e.g.,
\citealt{cesaroni2007,fallscheer2009,beltran2011}). Since collimated
outflows also exist in high-mass star formation (e.g.,
\citealt{beuther2002a,beuther2002d,zhang2005}), and these outflows
require stable inner accretion disks for the launching (e.g.,
\citealt{vaidya2009}), Keplerian disks are also expected around young
high-mass stars with masses $>$8\,M$_{\odot}$. The fact that the
latter are still observationally not detected in thermal line emission
indicates that these stable Keplerian structures are likely smaller
than the previous spatial resolution limit of thermal line emission on
the order of several 1000\,AU.  Interestingly, our target source
NGC7538\,IRS1 exhibits velocity signatures consistent with a Keplerian
disk observed in non-thermal maser emission on much smaller spatial
scales \citep{pestalozzi2004}. However, these maser features are
controversially discussed and are ambiguous (see next paragraph,
\citealt{debuizer2005,pestalozzi2009}).

Addressing this spatial resolution challenge, we studied one of the
best northern hemisphere high-mass accretion disk candidates
NGC7538\,IRS1 with the Plateau de Bure Interferometer (PdBI) in the
1.3\,mm wavelength window at $\sim 0.3''$ \citep{beuther2012c}. At the
approximate distance of $\sim 2.7$\,kpc
\citep{moscadelli2009,puga2010}, this corresponds to a linear
resolution of $\sim 800$\,AU.  NGC7538\,IRS1 had already previously
been extensively investigated. The central energy source is estimated
to be an O6 star with a mass of $\sim$30\,M$_{\odot}$ and a luminosity
of $\sim 8\times 10^4$\,L$_{\odot}$ (e.g.,
\citealt{willner1976,campbell1984,gaume1995b,pestalozzi2004,sandell2004,reid2005}).
While \citet{campbell1984b}, \citet{gaume1995b} and
\citet{sandell2009} report an ionized jet in the north-south direction,
\citet{minier2000} and \citet{pestalozzi2004,pestalozzi2009} present
the detection of CH$_3$OH class II masers at 6.7 and 12.2\,GHz, which is
indicative of an accretion disk perpendicular to the outflow. Partly
different interpretations arise from mid-infrared continuum imaging
\citep{debuizer2005c} that detect a disk-like structure in the
northeast-southwestern direction perpendicular to the molecular
outflow \citep{keto1991,davis1998}. Figure \ref{cont} shows the
various outflow/disk axes discussed in the literature so far.  Setting
high-spatial-resolution near-infrared speckle images of the region
into context with the existing data, \citet{kraus2006} propose
precession of the underlying disk-jet structure as the main reason for
observing different axis orientations. Furthermore,
\citet{hoffman2003} report high-spatial-resolution observations of
the rare H$_2$CO maser emission that is also consistent with a very
young disk candidate (cf.~\citealt{araya2007b}). In addition to the
proposed CH$_3$OH maser disk, \citet{minier2000} identified a few
additional CH$_3$OH maser positions, several of them approximately in
the east-west direction but one also in the south of the core
(Fig.~\ref{cont}). All these additional maser components are
blue-shifted with respect to the $v_{\rm{lsr}}$ and the southern
position is said to be associated with the ionized north-south
jet \citep{minier2001}.  \citet{qiu2011} observed red-shifted
absorption toward NGC7538IRS, which they interpret as infall motions
of the dense gas.

Resolving this region with the PdBI in the 1.3\,mm continuum emission,
as well as several spectral lines at $\sim$800\,AU resolution, the
source still remains one compact continuum core without evidence of
significant fragmentation \citep{beuther2012c}. Furthermore, in the
dense gas spectral lines, we identified a velocity gradient in the
northeast-southwest direction that is consistent with the mid-infrared
disk hypothesis of \citet{debuizer2005c}. However, the velocity
profiles are strongly affected by absorption against the strong
continuum, which made interpretating of velocity structures from a
potential disk almost impossible. Nevertheless, the absorption
profiles allowed us to estimate approximate mass infall rates on the
order of $10^{-2}$\,M$_{\odot}$\,yr$^{-1}$.

Based on these exciting results, we now aim to resolve and study this
promising massive disk candidate at the highest spatial resolution
possible in pre- and early-ALMA (Atacama Large Millimeter Array) time,
as well as in higher excited lines that may not be as affected by the
absorption than the lines of the previous studies. It should also be
noted that this important northern-sky star-forming region will never
be accessible with ALMA. Therefore, we observed NGC7538\,IRS1 at the
shortest wavelengths accessible with the PdBI at 843\,$\mu$m in its
most extended configuration. These observations resolve the submm
continuum and spectral line emission (HCN$(4-3)v_2=1$,
CH$_3$OH$(15_{1,14}-15_{0,15})$ and HCO$^+(4-3)$) at previously
unaccessible $0.2''\times 0.17''$ spatial resolution corresponding to
linear resolution elements of $\sim$500\,AU.  Questions we are
addressing with these observations are: What are the fragmentation
properties of the innermost core region? What are the rotational
properties of that entity?  How does the innermost outflow structure
relate to the rotational structure?

\section{Observations}
\label{obs}

\begin{figure}[ht!]
\includegraphics[width=0.48\textwidth]{21498f1.eps}
\caption{PdBI 843\,$\mu$m continuum image toward NGC7538\,IRS1. The
  full line contour levels start at $3\sigma$ values and continue in
  $1\sigma$ steps of 50\,mJy\,beam$^{-1}$ (black contours from 3 to
  9$\sigma$, white contours from 10 to to 14$\sigma$). The dashed
  contour shows the same negative levels. The thick full line presents
  the $4\sigma$ contour ($1\sigma\sim 29$\,mJy\,beam$^{-1}$) from the
  1.36\,mm data presented in \citet{beuther2012c}.  Several potential
  disk and outflow axes reported in the literature are presented
  (\citealt{davis1998,debuizer2005c,sandell2009,pestalozzi2004,pestalozzi2009,sandell2010},
  see Introduction for more details). The thick line presents the axis
  along which the position-velocity diagrams in Figure \ref{pv} are
  conducted. The northern and northwestern peaks submmN and submmNW
  are labeled, and the open star, the six-pointed star, and the white
  triangles mark the positions of the OH, H$_2$CO, and additional
  CH$_3$OH masers \citep{argon2000,hoffman2003,minier2001}. A
  scale-bar and the synthesized beam ($0.2''\times 0.17''$) are shown
  as well. The 0/0 position is the phase reference center in section
  \ref{obs}.}
\label{cont}
\end{figure}

NGC7538\,IRS1 was observed, together with NGC7538S, in a shared-track mode
in A configuration on February 27, 2012. The phase center of
NGC7538\,IRS1 was R.A (J2000.0)  23h\,13m\,45.360s, Dec.~(J2000.0)
61$^o$\,28$'$\,10.55$''$. Phase calibration was conducted with
regularly interleaved observations of the quasars 0059+581, 0016+731,
and 2320+506. The bandpass and flux were calibrated with observations
of 3C279. The absolute flux level is estimated to 20\% accuracy.  The
continuum emission was extracted from apparently line-free broad band
data obtained with the WIDEX correlator with four units and two
polarizations covering the frequency range from 354.16 to 357.77\,GHz.
The $1\sigma$ continuum rms for NGC7538\,IRS1 is 50\,mJy\,beam$^{-1}$.
To extract kinematic information, we put several high-spectral
resolution units with a nominal resolution of 0.312\,MHz or
0.26\,km\,s$^{-1}$ into the bandpass covering the spectral lines with
upper level energies $E_u/k$ between 43 and 1050\,K (Table
\ref{linelist}).  The spectral line rms for 1.0\,km\,s$^{-1}$ wide
spectral channels measured in emission-free channels, as well as
channels with emission, varies between 30 and 55\,mJy\,beam$^{-1}$.
The $v_{\rm{lsr}}$ is $\sim -57.3$\,km\,s$^{-1}$ (Gerner et al.~in
prep., \citealt{vandertak2000,sandell2010}).  The data were inverted
with a ``robust'' weighting scheme and cleaned with the Clark
algorithm. The synthesized beam of the final continuum and line data
is $\sim 0.2''\times 0.17''$ (PA 93$^{\circ}$). While NGC7538\,IRS1 is
extraordinarily strong in line and continuum emission, NGC7538S is
much weaker -- it was not detected in the spectral lines -- and even
imaging of the continuum was difficult. Therefore, we do not discuss
the NGC7538S data.

\begin{table}[htb]
\caption{Observed spectral lines}
\begin{tabular}{lrr}
\hline \hline
Freq. & Mol. & $E_u/k$ \\
(GHz) &       &  (K) \\
\hline
356.007152  & CH$_3$OH$(15_{1,14}-15_{0,15})$ & 278 \\
356.2555682 & HCN$(4-3)v_2=1$ & 1050 \\
356.734242  & HCO$^+(4-3)$ & 43 \\
\hline \hline
\end{tabular}
~\\
\label{linelist}
\end{table}

\section{Results and discussion}

\subsection{Fragmentation of the innermost core in the 843\,$\mu$m continuum emission}
\label{continuum}

Figure \ref{cont} presents the highest angular-resolution submm
continuum image (843\,$\mu$m or 356\,GHz) that has, to the authors'
knowledge, ever been obtained from a high-mass protostar and disk
region.  The synthesized beam of $0.2''\times 0.17''$ corresponds at
the given distance of 2.7\,kpc to a spatial resolution element of
approximately 500\,AU. For the first, therefore, time we resolve the
structures where not only the massive dense cores but also the
proposed embedded high-mass disks are expected to fragment (e.g.,
\citealt{krumholz2007a}).

\begin{figure*}[ht!]
\includegraphics[width=0.98\textwidth]{21498f2.eps}
\caption{The color scales in the left panels present the 0th moment
  (bottom, integrated intensity) and 1st moment (top, intensity
  weighted velocity) maps of the HCN(4--3)$v_2=1$ emission. In the
  middle and right panels, the color-scale shows the 0th and 1st
  moment maps (bottom and top, respectively) of
  CH$_3$OH$(15_{1,14}-15_{0,15})$. Black contours in all panels
  outline the dust continuum emission (Fig.~\ref{cont}) starting at
  the $3\sigma$ level and continuing in $2\sigma$ steps. The blue and
  red contours in the right panel show the blue- and red-shifted
  HCO$^+(4-3)$ emission integrated over the velocity regimes written
  above the panel. Contouring is done from 10 to 90\% of the
  respective peak emission. The white triangles present the additional
  maser positions by \citet{minier2000}, and a beam and scale bar are
  presented as well. The CH$_3$OH 1st moment map also marks the axis
  along which the position-velocity cuts in Fig.~\ref{pv} are
  conducted.}
\label{moments}
\end{figure*}

While the lower resolution 1.36\,mm image in \citet{beuther2012c}
consisted mainly of an unresolved point source with only very little
extended emission at low intensities, the new 843\,$\mu$m data now
reveal substructure within the inner $\sim$3000\,AU of the region. In
addition to spatially resolving the central peak into an elongated
structure with a subpeak about $0.3''$ ($\sim 900$\,AU) north of the
main peak (Fig.~\ref{cont}), there appears to be a secondary structure
toward the northwest of the main peak. While the arm-like structure is
at the 3-4$\sigma$ level, the northwestern peak of that arm (offset
$-0.11''/0.36''$ or $\sim 1300$\,AU, labeled submmNW in
Fig.~\ref{cont}) is above $5\sigma$. The lowest $4\sigma$ contour of
the previous 1.36\,mm data ($1\sigma\sim 29$\,mJy\,beam$^{-1}$,
\citealt{beuther2012c}) shows only a weak extension in that direction.
The peak 843\,$\mu$m flux from submmNW is
$\sim$0.27\,mJy\,beam$^{-1}$, and assuming a $\nu^4$ flux dependence
at (sub)mm wavelength, which translates into a 1.36\,mm flux of
$\sim$40\,mJy\,beam$^{-1}$. This is below the $2\sigma$ level of the
previous 1.36\,mm data, so it explains the non-detection at the longer
wavelengths. The detection of fragmenting substructure in the dense
core/disk at the shorter wavelengths shows the power of this
wavelength range.

The peak and integrated (above $3\sigma$ level) 843\,$\mu$m fluxes
extracted from Fig.~\ref{cont} are 0.74\,Jy\,beam$^{-1}$ and 3.38\,Jy,
respectively. At the given spatial resolution, the peak and 3$\sigma$
fluxes of 0.74 and 0.15\,Jy\,beam$^{-1}$ correspond to brightness
temperatures from the peak to the edge between 219 and 51\,K.
\citet{reid2005} report an 850\,$\mu$m single-dish continuum peak flux
of 18.1\,Jy\,beam$^{-1}$, which implies that our interferometer
observations filter out approximately 80\% of the total flux. To
calculate masses and column densities, it is important to estimate the
free-free contribution to the total flux measured at the given
wavelengths. While the free-free emission has approximately a $\nu^2$
dependence in the optically thick regime, it turns almost flat
($\nu^{-0.1}$) in the optically thin regime. As a result, if one knows the
turnover frequency between the two regimes such an estimate is
relatively easy. However, that turnover frequency has not been determined
yet for NGC7538\,IRS1. \citet{sandell2009} compiled the cm wavelength
fluxes and find rising fluxes up to 43.4\,GHz where they measure
a flux of $\sim$430\,mJy toward the central elongated but still
compact core (size $0.2''\times 0.14''$, smaller than our synthesized
beam). This value can be considered as a lower limit of the free-free
contribution even at submm wavelengths.  But because the spectral
energy distribution has not reached the optically thin regime at that
wavelength yet, giving an upper limit is difficult. In our previous
1.36\,mm study we assumed 1\,Jy as a free-free flux contribution;
however, that is obviously too high because we only measure
0.74\,Jy\,beam$^{-1}$ peak flux in our new submm PdBI data.  As an
approximation, we assume 0.5\,Jy as a free-free flux contribution at
843\,$\mu$m, which results in a dust-related peak and integrated fluxes
at that wavelength of 0.24\,Jy\,beam$^{-1}$ and 2.88\,Jy,
respectively. Interestingly, after correcting for the free-free
emission, the dust related 843\,$\mu$m peak flux from the central peak
is very close to that measured from the northern peak (submmN) with
$\sim$0.26\,mJy\,beam$^{-1}$ and the northwestern extension peak
(submmNW) with $\sim$0.27\,mJy\,beam$^{-1}$. While even submmN and
submmNW may make free-free contributions to the measured flux, based
on the published cm data, this potential contribution should be very
small \citep{sandell2009}.

Assuming optically thin emission of dust at submm wavelength at an
approximate temperature of 245\,K \citep{qiu2011} with a dust opacity
$\kappa\sim 1.8$\,cm$^2$\,g$^{-1}$ (extrapolated from
\citealt{ossenkopf1994} for densities of $10^6$\,cm$^{-3}$ and dust with
thin ice mantles) and a gas-to-dust mass ratio of 186
\citep{jenkins2004,draine2007}, the integrated flux corresponds to a
total mass of the submm structure of $\sim$11\,M$_{\odot}$. Using the
peak fluxes to estimate the mass contributions of resolved fragments
(central submmN and submmNW), they have similar values with 0.9, 1.1,
and 1.0\,M$_{\odot}$, respectively.
The gas column densities toward the central peak, as well as submmN and
submmNW, are approximately the same with $0.9\times 10^{25}$,
$1.0\times 10^{25}$, and $1.0\times 10^{25}$\,cm$^{-2}$, respectively.
This corresponds to very high visual extinction values around
$10^5$\,mag. For comparison, assuming ISM dust properties
\citep{mathis1977} in the classical \citet{hildebrand1983} picture the
masses and column densities would be higher with values of
$\sim$25\,M$_{\odot}$, $2.0\times 10^{25}$, $2.1\times 10^{25}$, and
$2.2\times 10^{25}$\,cm$^{-2}$, respectively.  Independent of the
assumed dust properties, the detection of a central infrared source
(e.g., \citealt{puga2010}), in spite of such extremely high gas
column density and extinction values, indicates that the outflow is
likely to be aligned not to far off the line-of-sight excavating a
cavity through which we can peer into the center (see section
\ref{outflow}).

In addition to the fragmenting structures on 1000\,AU scales, the
extremely high spatial resolution of this continuum map also reveals
an elongation of the central peak around NGC7538\,IRS1. At the
$>10\sigma$ level, the 843\,$\mu$m emission appears elongated along an
axis approximately inbetween the north-south jet axis and the
northeast-southwest mid-infrared and molecular disk axis marked in
Figure \ref{cont}. This orientation of the elongation reflects the
likely situation that the submm emission receives contributions from the
assumed underlying dusty disk, as well as from the ionized jet.
However, we cannot exclude that the elongation could also be due to an
unresolved binary. \citet{kraus2006} do not find any equal brightness
binary at their spatial resolution limit of 70\,mas, but their
proposed precession model requires a very close and unresolved binary
component. Furthermore, the data reveal elongated and more extended
emission $\sim 0.3''$ east of the main peak. While this emission can
be part of the smoother envelope emission, it may also host another
unresolved subsource in the region.

The fragmenting core structure is consistent with - if not a
prerequisite for - the observed high degree of multiplicity and
Trapezia systems in high-mass star formation (e.g.,
\citealt{zinnecker2007}). While fragmentation can also be suppressed,
for example, by magnetic fields (e.g., \citealt{commercon2011}),
recent hydrodynamical simulations of collapsing gas clumps predict the
fragmentation of the rotating cores/disks and even competitive
accretion between the different subfragments within the disk
\citep{krumholz2009,peters2010b}.  The model-predicted fragmentation
scales of the inner core/disk structures range between several 100 and
a few 1000\,AU, resembling the observed structures fairly closely.

\begin{figure}[ht!]
\includegraphics[width=0.49\textwidth]{21498f3a.eps}
\includegraphics[width=0.49\textwidth]{21498f3b.eps}
\includegraphics[width=0.49\textwidth]{21498f3c.eps}
\includegraphics[width=0.49\textwidth]{21498f3d.eps}
\caption{The top three continuum-subtracted spectra are extracted for
  HCN, CH$_3$OH and HCO$^+$ toward the central peak position (offset
  $0.1''/-0.2''$). The bottom spectrum shows the HCO$^+$ spectra from
  the blue- and red-shifted outflow peak positions presented in
  Fig.~\ref{moments} (offsets positions $0.33''/0.18''$ and
  $-0.18''/-0.48''$, respectively).}
\label{spectra}
\end{figure}

\subsection{Gas kinematics}

The spectral line data also allow us to investigate the gas kinematics
of the different components in more detail. Figure \ref{moments} gives
an overview of the HCN$(4-3)v_2=1)$, CH$_3$OH$(15_{1,14}-15_{0,15})$,
and HCO$^+(4-3)$ results. While we show for HCN$(4-3)v_2=1$ and
CH$_3$OH$(15_{1,14}-15_{0,15})$ zeroth (integrated intensity) and
first moment maps (intensity-weighted velocities), the blue- and
red-shifted high-velocity gas is presented for HCO$^+(4-3)$. Figure
\ref{spectra} additionally shows the spectra of all three lines
extracted toward the continuum peak, as well as the HCO$^+(4-3)$
spectra toward the blue- and red-shifted outflow peak positions.

While both high-density tracers -- HCN$(4-3)v_2=1$ and
CH$_3$OH$(15_{1,14}-15_{0,15})$ -- clearly show the
northeast-southwest velocity gradient of the underlying rotating
core/disk structure on scales of approximately 3000\,AU, it is
interesting that the highest excited HCN$(4-3)v_2=1$ line with an
upper energy level $E_u/k$ of 1050\,K still exhibits the central
absorption features. Considering the peak brightness temperature of
the continuum emission of 219\,K, this implies that the beam-averaged
excitation temperature of the spectral line has to be lower than that.
At the high densities within the core, the same applies to the
beam-averaged gas kinetic temperatures. The $E_u/k=278$\,K
CH$_3$OH$(15_{1,14}-15_{0,15})$ line is among the few lines that do
not show any absorption at high spatial resolution.  From the suite of
lines presented in \citet{beuther2012c}, that covers a broad range of
energy levels between 21 and 326\,K, only the optically thin
methyl-cyanide isotopologue CH$_3^{13}$CN did not show any prominent
absorption feature. Since the CH$_3$OH$(15_{1,14}-15_{0,15})$ line is
very strong and probably not optically thin, it does not seem to be an
optical depth effect here.  Why this line does not show up in
absorption is not exactly clear yet. However, it is known that many
CH$_3$OH transitions are potential masers. One condition for the
inversion population for masers is a negative excitation temperature.
On the way to inversion population, the excitation temperature first
asymptotically rises to high $T_{\rm{ex}}$ (e.g.,
\citealt{stahler2005}, Fig.~14.6) before it inverts and becomes
negative. Hence, even in the non-masing state, a molecule like
CH$_3$OH may more easily exhibit high excitation temperatures and thus
less absorption than most other molecules.  Independent of that, the
CH$_3$OH emission line is very useful for studying the rotational
properties of the core without absorption artifacts.

\subsubsection{Rotational properties}

While a rotating inner envelope and/or disk structure is already
evident from the first moment map (Fig.~\ref{moments}), to investigate
whether a Keplerian accretion disk can be identified with the new
data, Figure \ref{pv} presents position-velocity cuts for
HCN$(4-3)v_2=1)$ and CH$_3$OH$(15_{1,14}-15_{0,15})$ along the
northeast-southwest axis most likely representing the orientation of
the proposed embedded disk. This axis is not exactly aligned with the
extension of the continuum emission (Sec.~\ref{continuum}), but it is
the axis of the strongest velocity gradient (Figs.~\ref{cont} \&
\ref{moments}).  Although we identify a clear velocity gradient across
the core, thereby confirming its general rotation, the
position-velocity diagram is not consistent with Keplerian rotation,
but the data instead exhibit sub-Keplerian motions of the gas. To
visualize this, Fig.~\ref{pv} shows the position-velocity signatures
one would expect for a central 30\,M$_{\odot}$ and 8\,M$_{\odot}$
star. Obviously, none of these rotation curves fits the observations,
which implies that we still miss clear signatures of a Keplerian
accretion disk around genuine high-mass young stellar objects.

While Keplerian disks have been identified and studied intensively for
low-mass TTauri stars (e.g., \citealt{simon2000}), Keplerian rotation
has been identified only in a few cases around early B-type stars
(e.g., AFGL490 or IRAS\,20126, \citealt{schreyer2002,cesaroni2005}).
However, in the high-mass regime mainly larger scale rotating toroids
have been found (e.g., \citealt{cesaroni2007,fallscheer2009}).
Recently, a large PdBI survey of several low-mass class 0 sources did
not identify any Keplerian disk on scales larger than 50\,AU
(\citealt{maury2010}, Maury et al.~in prep.). This implies that the
real Keplerian disks around very young low-mass protostars have to be
very small in size.  Extrapolating this picture to the high-mass
sources, we have also not found Keplerian disks on scales $> 500$\,AU.
One should keep in mind that the rotating envelope mass of around
11\,M$_{\odot}$ is a significant fraction of the reported stellar mass
of 30\,M$_{\odot}$ (which is an upper limit because the mass estimates
based on the luminosity do not properly take the potential accretion
luminosity into account). Since a requirement for Keplerian rotation
is that the disk mass is negligible compared to the mass of the
central object, real Keplerian signatures may not even be expected on
these larger scales.  Since in both the low-mass and high-mass cases,
collimated outflows are known that indicate stable disks for their
launching, in the high-mass case we also have to achieve better
spatial resolution and search for these entities on still smaller
scales. Small inner Keplerian disks are also consistent with
near-infrared spectral line observation results (e.g.,
\citealt{thi2005,wheelwright2010,ilee2013}.) In principle, one could
fathom such a small inner accretion disk also in the ionized gas,
however, high-spatial-resolution recombination line studies of this
region also exhibit the north-south jet-structure with very broad
recombination lines \citep{gaume1995b}. These are more
straightforwardly interpreted in the framework of an outflow/wind
model for the ionized gas.

It is interesting to note that the additional blue-shifted CH$_3$OH
maser components that are not part of the proposed Keplerian disk but
found a bit offset (Figs.~\ref{cont} and \ref{moments},
\citealt{minier2000,minier2001}) are spatially and velocity-wise
correlated with the rotating gas observed in HCN and CH$_3$OH and less
with the inverse velocity-structure seen in HCO$^+$. This strongly
indicates that the masers are not part of the outflow but of the inner
rotating core.

\begin{figure*}[ht]
\includegraphics[width=0.98\textwidth]{21498f4.eps}
\caption{Position-velocity diagrams for HCN(4--3)$v_2=1$ (left)
  CH$_3$OH$(15_{1,14}-15_{0,15})$ (right) along the
  northeast-southwest, mid-infrared and molecular axis shown in
  Fig.~\ref{cont}.  The full and dashed lines mark the rotation curves
  for embedded 30 and 8\,M$_{\odot}$ objects, respectively. The
  $v_{\rm{lsr}}$ is shown as well.}
\label{pv}
\end{figure*}

\subsubsection{Infall rates}
\label{infall}

The HCN$(4-3)v_2=1$ spectrum extracted toward the submm peak positions
exhibits clear blue- and red-shifted absorption signatures.
\citet{knez2009} found similar spectral absorption signatures in
spectral line observations at mid-infrared wavelengths, and they
interpret their data in the framework of absorption from a nearly
edge-on disk. We think that the expected underlying embedded
disk-structure is currently unlikely to be too close to edge-on but
has to have a considerable inclination angle mainly for two reasons:
(1) If a flattened disk-like structure were fully edge-on, the central
source would be highly extincted and no or barely any emission would
be expected to escape at near-infrared wavelengths. In contrast to
that picture, near-infrared observations detect a central source
(e.g., \citealt{puga2010}). While the infrared emission could also in
principle be due to scattered light from the outflow cone (e.g.,
\citealt{kraus2006}), a simpler way to explain such a detection in the
presence of high column densities and extinctions as reported in
section \ref{continuum} is that one observes the region at least at
medium inclination through the cleared-out outflow cavity.  (2)
Furthermore, the velocity structure observed in HCO$^+$(3--2) (see
section \ref{outflow}) indicates that we have to look at least to some
degree into the cavity of the outflow. An additional aspect of the
whole region to be considered is the strong precession of the
disk-outflow system proposed by \citet{kraus2006}. While such
precession cannot only change the projected angle of the outflow on
the plane of the sky, it would also change the inclination to the
observer.  Therefore, in this precession model it is possible that the
outflow cone is closer to the line-of-sight during different
time steps in the evolution of the system.

Therefore, we favor a geometry with the outflow orientation being
closer to the line of sight where any flattened disk-like structure
has to be closer to face-on. Deriving an exact inclination angle is
not possible with the given data. In this framework, the blue-shifted
absorption should stem from outflowing gas, whereas the red-shifted
absorption indicates infalling gas.  Observing this infall in a line
with $E_u/k$ higher than 1000\,K implies that the infall continues
down to the innermost region around the star.  Although it is unclear
what fraction of the gas will finally be accreted, infall rates
estimated from these signatures should give an upper limit for the
actual accretion rates.

Assuming a spherical infall geometry, one can estimate mass infall
rates via $\dot{M}_{\rm{in}} = 4\pi r^2 \rho v_{\rm{in}}$ where
$\dot{M}_{\rm{in}}$ and $v_{\rm{in}}$ are the infall rate and infall
velocity, and $r$ and $\rho$ the core radius and density (see also
\citealt{qiu2011,beuther2012c}). We estimate the radius as $r=250$\,AU,
which is half our spatial resolution limit, corresponding well to the
area where absorption is present (Figure \ref{moments}, left
panels). The estimated density $\rho\sim 1.2\times 10^9$\,cm$^{-3}$
results from assuming that the peak column density derived above is
distributed along the line-of-sight at our spatial-resolution limit,
i.e., 500\,AU. The infall velocity can be estimated to
3.2\,km\,s$^{-1}$, which corresponds to the difference between the most
red-shifted absorption at $\sim -54.1$\,km\,s$^{-1}$, and the
$v_{\rm{lsr}}\sim -57.3$\,km\,s$^{-1}$. With these numbers, we derive
an infall rate of $\dot{M}_{\rm{in}} \sim 3.6\times
10^{-3}$\,M$_{\odot}$\,yr$^{-1}$.
This estimate is approximately a factor 20 lower than the infall rates
derived previously from the 1.36\,mm line data \citep{beuther2012b}.
The main difference stems from the higher spatial resolution of the
new data that enters the equation for $\dot{M}_{\rm{in}}$ through
$r^2$. Adding in the higher upper level energy of the HCN$(4-3)v_2=1$
line, the new value should resemble the actual accretion rates better
than the previous estimate.  To additionally improve our 1D spherical
infall estimate into a 2D disk geometry, we follow the arguments given
in \citet{beuther2012b}: Considering that the accretion does not occur
in a spherical mode over $4\pi$ but rather along a flattened disk
structure with a solid angle of $\Omega$, the actual disk infall rates
$\dot{M}_{\rm{disk,in}}$ should scale like
$\dot{M}_{\rm{disk,in}}=\frac{\Omega}{4\pi}\times \dot{M}_{\rm{in}}$.
Based on the simulations by \citet{kuiper2012} and R.~Kuiper
(priv.~comm.), the outflow covers approximately an 120\,degree opening
angle, and the disk 60\,degree (to be doubled for the north-south
symmetry). Since the opening angle does not scale linearly with the
surface element, full integration results in $\sim$50\% or $\sim 2\pi$
of the sphere being covered by the disk.  This then results in disk
infall rates of $\dot{M}_{\rm{disk,in}}\sim 1.8\times 10^{-3}$
\,M$_{\odot}$\,yr$^{-1}$, which is still very high and in the regime
of accretion rates required to form high-mass stars (e.g.,
\citealt{wolfire1987,mckee2003}).

\subsubsection{Outflow properties}
\label{outflow}

The blue- and red-shifted outflow signatures in the H CO$^+$(-3--2)
line in the northeast-southwest direction come as a surprise at first
sight. They appear aligned with the northeast-southwest axis of the
rotating structure, almost perpendicular to the CO and mid-infrared
outflow and still at a considerable angle to the ionized jet. The
facts that the HCO$^+$ velocities are significantly higher than the
rotational velocities measured in this direction by the CH$_3$OH and
HCN lines, as well as the inversion of blue- and red-shifted gas with
respect to the rotational structure, strongly indicate that the
HCO$^+$ emission traces different gas than do the other presented
lines.

Additional information can be extracted from the spectra taken toward
the blue- and red-shifted peak positions (Fig.~\ref{spectra}). These
spectra clearly show the blue- and red-shifted line wings, but both
spectra exhibit additional emission components. The spectrum toward
the blue-shifted peak position has another component at $\sim
-51.3$\,km\,s$^{-1}$ that is red-shifted with respect to the
$v_{\rm{lsr}}$. Correspondingly, the spectrum extracted from the
red-shifted peak exhibits an additional emission component at $\sim
-78.6$\,km\,s$^{-1}$ that is extremely blue-shifted compared to the
$v_{\rm{lsr}}$. Combining these two spectra, we see that both lobes
exhibit blue- and red-shifted emission. In an outflow scenario, this
indicates that the outflow is aligned almost along the line-of-sight
and that emission from both outflow lobes is found within the same
observational beams. The projected molecular HCO$^+$ outflow
geometry indicated by Fig.~\ref{moments} thus does not really reveal the
actual outflow geometry, but the outflow has to be aligned closer to
the line-of-sight. This agrees well with the fact that we see
infrared emission from a central object (e.g.,
\citealt{linz2009,puga2010}) from a region with such high column
densities, hence visual extinction (see section \ref{continuum})
that should prohibit any emission at short wavelengths. With an
outflow cone along the line-of-sight, the near-infrared emission can
easily escape and reach the observer (e.g.,
\citealt{hofner2001,linz2005}).

As already discussed in section \ref{infall}, the proposed precession
of the system has to be taken into account as well \citep{kraus2006}.
This implies that the inclination of the outflow cone with respect to
the line-of-sight can vary during different time steps in the
evolution of the system.

\section{Conclusions}
\label{conclusion}

These so far highest spatial-resolution submm observations of the
dense dust and thermal gas around a high-mass protostar reveals
several exciting results. For the first time, we have resolved
fragmentation properties of the rotating inner core with at least
three subsources within the inner 3000\,AU.  This is consistent with
the high degree of multiplicity found for high-mass stars. The region
also resembles structures found recently in hydrodynamical simulations
of collapsing gas clumps. In addition to the fragmentation results,
the data also clearly outline the importance of going to shorter
wavelengths to identify such fainter structures because the $\nu^4$
frequency dependence strongly outweights the poorer atmospheric
conditions at shorter wavelengths.

Identifying red-shifted absorption signatures of infall motions from a
high-excitation temperature ($E_u/k\sim 1050$\,K) tracer like the
HCN$(4-3)v_2=1$ line on scales $\leq 500$\,AU from the central
protostars allows us to estimate infall rates around $1.8\times
10^{-3}$\,M$_{\odot}$yr$^{-1}$. Although it is unclear what fraction
of the gas actually falls on the star, such inner core/disk infall
rates are among the best proxies of the actual accretion rates we can
get at that early evolutionary stage.

The outflow exhibits blue- and red-shifted emission on both sides of
the central object. This can only be explained by an outflow cone
opening almost along the line-of-sight, hence emitting blue- and
red-shifted gas within the same observational beam. Such a
line-of-sight outflow is also prerequisite for the simultaneous
detection of extremely high visual extinction values (on the order
$10^5$\,mag) and at the same time infrared emission from the central
object.

Collimated and jet-like outflows are usually considered to require
stable central, most likely Keplerian disks, and the search for these
objects is still open.  Although we clearly identify rotational
signatures of the core on $\sim$3000\,AU scales, even at our
resolution limit of 500\,AU we are not able to identify Keplerian
velocity signatures. The difficulty to identify disks during early
evolutionary stages has also recently been reported for low-mass class 0
sources (Maury et al.~in prep.).  Identifying and studying these low-
and high-mass accretion disks during the earliest evolutionary stages
remains one of the exciting topics in high-mass star formation for the
coming years.

While these observations are at the edge of the capabilities of
currently existing (sub)mm interferometers, they outline the immense
potential of ALMA and NOEMA in that field.

\begin{acknowledgements}
  We would like to thank the IRAM staff, in particular Jan Martin Winters,
  for all support during the observation and data reduction process.
  Furthermore, we acknowledge the referee's report and comments
  that improved the paper.
\end{acknowledgements}

\input{21498.bbl}

\end{document}

redpajama_set_name: RedPajamaArXiv


text:
Voter Privacy: What Canada can learn from abroad
Why are election-related issues such as voter privacy not more widely discussed during election time? Sabrina Wilkinson compares the access Canadian political parties have to voter data compared to their international counterparts.
Sabrina Wilkinson
Canada's Chief Electoral Officer Stephane Perrault tours the Elections Canada distribution centre in advance of the upcoming federal election, in Ottawa, Ontario, Canada, August 29, 2019. REUTERS/Chris Wattie
By: Sabrina Wilkinson
researcher and writer
Is global cooperation on social media governance working?
2018 elections put digital protection measures to the test
Last month, just a day before the formal start of Canada's federal election campaign, the CBC reported that the official websites of 99 Canadian members of parliament have trackers that can collect visitors' data and target them with political advertisements. The tools can catalogue users' information, such as their IP addresses, and use that data to identify individuals and present them with tailored content online, including on social media sites like Facebook.
The use of website trackers isn't illegal, but, especially in the lead up to the October 21 vote, it does highlight the relevance of a dialogue surrounding privacy and political parties. Since the writ drop on September 11, parties have heightened efforts to collect voter information and target Canadians with personalized messages. In some cases, inadequate data protection efforts have led to worrying privacy violations, including the inadvertent publication of voters' personal details online.
Canadian political parties' management of personal data is largely unregulated in comparison to the collection and use of such information in the private and public sectors. And the operation of these tools is inconsistent with statements from the Privacy Commissioner of Canada, Daniel Therrien. "Canadians expect and deserve to have their privacy rights respected as they exercise their democratic rights," he said earlier this year.
Therrien has proposed that Canadian political parties be governed by privacy legislation based on international standards and overseen by an independent third party. At the provincial and territorial level, British Colombia is the only jurisdiction that regulates parties' personal data practices, and the province's courts have faced challenges from national parties on their authority to do so.
In an increasingly digital world, lax privacy protections for voters can limit the electorate's trust in political parties and candidates, and weaken the strength of democratic institutions. Such concerns should prompt a look outside Canada's borders to explore how voter privacy is protected in other countries, and what lessons Canadian legislators can learn from their international counterparts.
Lessons from the EU: Security, enforcement, and voter rights
In the European Union, the General Data Protection Regulation (GDPR), which came into effect in May 2018, has strengthened the bloc's protections around personal data. These obligations extend to European and national parties, which are required to process personal information "lawfully, fairly and in a transparent manner, for specified purposes only." Many of the ideals embedded in this regulation, including parties' responsibilities around security, access and transparency, are worthy of study.
For one, the GDPR obliges parties to promptly notify users of data breaches that are "likely to result in a high risk to [individuals'] rights and freedoms," use secure operational systems and process information according to specific conditions, among other responsibilities. Voters are also granted strong rights under the legislation, including the right to access their data, to request the deletion of their data under certain circumstances and to have inaccurate data corrected.
To be sure, this legislation hasn't been uniformly interpreted across the union. The GDPR allows some flexibility in member states' application of the EU regulation into national law, and this leniency has been exploited by some countries. Open Rights Group, a digital rights organization based in the United Kingdom, highlights, for instance, that Romania allows political parties "to process personal data from special categories without explicit consent and without implementing appropriate safeguards." The group also points out concerning allowances in Spanish and British laws.
Canadian political parties' management of personal data is largely unregulated in comparison to the private and public sectors.
And the GDPR faces other threats, including, as the University of Victoria's Colin Bennett puts it, "continuing pressure from technological, political, and social forces that will demand the freer flow of information about the behaviours and attitudes of voters." Yet, broadly, the regulation offers modernized rules for an increasingly connected citizenry and in ways that give voters more control over how their data is collected, stored and used. Canadian law makers should take note.
The EU can also be lauded for its tough approach to oversight and rule-breaking in the area of voter privacy, both with respect to the GDPR and other privacy rules. For example, according to recent legislation from the bloc, European political parties can face sanctions for trying to influence the outcome of European Parliament elections with illicitly collected data. An independent authority would verify and penalize potential violations.
In Canada, by contrast, the Privacy Commissioner's Office has no authority over the operations of political parties, and Elections Canada is under no obligation to enforce parties' privacy policies.
Taking caution from the approaches in Australia and the US
But there are also countries whose regulatory approaches Canada shouldn't emulate, like the United States and Australia. For nearly 20 years, Australia's political parties have been exempt from federal privacy legislation "on the basis of the importance of freedom of political communication." The arrangement has regularly come to a head over the years, including in one recent example.
In Feburary 2019, Australia's cyber intelligence agency discovered that a state actor had hacked the networks of the country's three major political parties, just months before a federal election. The hacker, which was later identified as China, gained access to policy papers and "private email correspondence between lawmakers, their staff and other citizens." Critics charged that the incident was in part due to parties' permissive security measures and highlighted the potential for other hacks to go undisclosed, given that parties are not required to publicize breaches.
The situation also underscored the prospect that foreign hackers could use stolen voter data to interfere with Australia's democratic processes. Given that Canada's political parties are similarly exempt from federal privacy laws, these anxieties shouldn't be overlooked.
In the US, experts suggest that political parties' lax data protection practices are an upshot of the lack of broad privacy laws, the existence of strong freedom of speech and association protections, and permissive campaign finance rules. This confluence of factors has contributed to the immense prevalence of microtargeting in US political campaigns, alongside other troubling uses of personal data.
In politics, microtargeting describes parties' use of voters' personal information to segment the populace into groups, which can then be targeted with tailored political content. The practice has been at the heart of a number of privacy scandals in the US in recent years. The most prominent of these is the extensive use of microtargeting by data profiling company, Cambridge Analytica, which, alongside other projects, worked on the 2016 Trump campaign. While in operation, the firm collected data from more than 87 million people globally, including about 620,000 Canadians.
While microtargeting is used by some parties in Canada, it's nowhere near as pervasive a strategy. Yet, recent examples, coupled with the constrained limitations on Canadian political parties' activities, could signal an increase in the practice.
The case for reform in Canada
One of the greatest challenges facing an expansion to the privacy rules governing Canada's political parties is that politicians who benefit from limited regulations are effectively gatekeepers to such legislative changes. And certainly, many political candidates may rightly suggest that access to citizens is a critical part of an informed and healthy democracy. But recent violations of voter privacy by parties in Canada, and around the world, show that this access needs to be duly checked. A balance between access to, and protections for, citizens is necessary.
Alternatively, Canadian legislators should consider the opportunities provided by such reform. In December 2018, a survey from Nanos Research found that 36 percent of Canadians are concerned about how political parties use voters' personal information, and 37 percent are somewhat concerned. Advocating for strengthened legislation in this area would only be a boon to federal party platforms, especially in such a crowded field.
Some have made the case for stronger oversight. The Green Party of Canada includes the issue in its 2019 platform document, which affirms that parties should follow the Privacy Act, the legislation that sets out the privacy rules for the public sector, "without exception." The three major federal parties, meanwhile, haven't made any similar affirmations.
Applying learnings from international counterparts, and from the EU especially, should be a first step in the reform process. Earlier this year, Canada's Office of the Privacy Commissioner and Chief Electoral Officer outlined 10 principles to guide Canadian political parties' privacy polices, including consent, accountability, limited collection and use of data, and openness. These ideals, many of which are championed by the GDPR, should also inform reform efforts. At the same time, the approaches of countries like the US and Australia, which have weak regulations and histories of privacy contraventions, should serve as warnings.
There's limited time for political candidates running in the upcoming federal election to bring these lessons to Canadians' doorsteps — but even if changes are not made in this campaign, they can certainly guide elections to come.
Journalism in Canada has suffered a devastating decline over the last two decades. Dozens of newspapers and outlets have shuttered. Remaining newsrooms are smaller. Nowhere is this erosion more acute than in the coverage of foreign policy and international news. It's expensive, and Canadians, oceans away from most international upheavals, pay the outside world comparatively little attention.
At Open Canada, we believe this must change. If anything, the pandemic has taught us we can't afford to ignore the changing world. What's more, we believe, most Canadians don't want to. Many of us, after all, come from somewhere else and have connections that reach around the world.
Our mission is to build a conversation that involves everyone — not just politicians, academics and policy makers. We need your help to do so. Your support helps us find stories and pay writers to tell them. It helps us grow that conversation. It helps us encourage more Canadians to play an active role in shaping our country's place in the world.


text:
Hello there. Welcome to another segment of Chazz Radio.
I came across an interesting article and I thought that you should be interested too, that is if you're interested in whether our president has the right to be the president.
I'm going to read to you from the article and I will also provide the link to the article.
It's actually a video and a very interesting one although it doesn't surprise me.
The Secret Service, FBI and CIA are carefully watching a certain individual whose code name is "Renegade." The following is from his dossier.
Name - Barack Hussein Obama.
Alias -Barry Soetoro.
Born -1961
Politics -Socialist
Status - Unclear
Father - Barack Hussein Obama senior.
Born - Colony of Kenya
Status -British subject
Politics -communism
Religion -Muslim
Mother -Stanley Ann Dunham
Born - Wichita Kansas
Status - U.S. citizen
Politics - Progressive
Religion - Secular Humanism
Obama's parents meet in a Russian language class at the university of Hawaii in 1960.
They get married on February 2 1961. Barack is born later that year.
They separate when Barack is two years old and divorce in 1964.
Place of birth - allegedly Hawaii
Hospital of birth -allegedly Kapi' olani
Delivering Dr. -unknown
Birth certificate -unavailable
He will not release a copy of his original birth certificate for examination by the public or the authorities.
Obama's mother then marries Indonesian student Lolo Soetoro, also a Muslim.
Soetoro is recalled to Indonesia by Suharto in 1967. Mother and son follow Lolo to Indonesia soon after.
Barack is then adopted by Lolo.
Obama is renamed Barry Soetoro and at the age of six he is enrolled in the first grade.
According to his records, he is a citizen of Indonesia and his faith is Islam.
There's no record that Barry Soetoro ever officially changed his name back to Barack Obama, so he may now be operating under a false identity.
There is no record that Barry Soetoro ever officially changed his citizenship back to American, so he may currently remain an Indonesian citizen.
In 1971 at the age of 10, Barry Soetoro is sent by his mother to live with his maternal grandparents in Hawaii.
Barry's grandparents are Communists. They specifically enrolled their daughter in the Mercer Island High School near Seattle when the chairman of the school board there testifies to being a Communist.
While growing up in Hawaii, he meets Frank Marshall Davis: a journalist, poet, self -avowed Communist, labor union activist and friend of his grandparents. Davis has been under investigation by the FBI and Congress H U A C.
He becomes Obama's Mentor.
Obama admits to attending socialist conference's and coming into contact with Marxist literature.
Karl Marx advocated the redistribution of wealth and endorsed the organization known as Socialist International. Communism was based on the writings of Marx.
Barry maintains his relationship with Frank Marshall Davis through grade 12.
Barry leaves Hawaii and allegedly attends Occidental College in Los Angles. Only the accounts of his friends proved that he was there.
He has never released any transcripts, writings or record of his time at Occidental.
It has been alleged that while at Occidental, he used the name " Barry Soetoro" and was registered as a student from Indonesia.
California assembly records suggest that he received a state grant as a foreign exchange student from Indonesia.
In his book " Dreams From My Father", Obama said this of his days at Occidental...
I chose my friends carefully, the more politically active black students... The Marxist professors and structural feminists.
Barry's friends at Occidental include three Pakistanis named Wahid Hamid, Sohale Siddiqi and Mohammed Hassan Chandoo.
Obama and Hamid travel to Pakistan in 1981. The purpose of their trip remains unknown. Mohammed Hassan Chandoo later becomes a "Bundler" for Obama raising as much as $100,000.
After two years Barry leaves Occidental. He allegedly attends Columbia University in New York City. Only the accounts of friends and professors prove that he was there. He has never released any transcripts, writings or records of his time at Columbia.
He allegedly attends Harvard University, graduates with a JD and becomes president of the Harvard Law Review. He has never released any of the transcripts, writings or records of his time at Harvard.
He goes to Chicago, becomes an Atty., and begins work as a community organizer. When he is sworn in as an Illinois Atty., and is asked under oath if he had used any other names, he responds," none". By doing so, he defrauds The State Bar of Illinois and perjures himself.
He reads "Rules For Radicals" written by Saul Alinsky and embraces the concepts whole-hardheartedly. Mike Kruglik had this to say about Obama's mastery of Alinsky's methods: "He was a natural the undisputed master of agitation who could engage a roomful of recruiting targets".
He meets with Bill Ayers an unrepentant terrorist and co-founder of the Weather Underground.
In the 1960s this group claimed responsibility for a dozen bombings.
From 1995 to 1999 Obama is Chairman of the Chicago Annenberg Challenge, a project designed to reform Chicago public schools.
Bill Ayers writes the initial grant application. A grant is issued for $49.2 million. Matching donors increase that amount even more. The funds are spent but not well accounted for, and interestingly public schools do not improve.
He starts his political career in the home of Bill Ayers, who says he didn't do enough during the sixties.
He joins the New Party, formed by the Democratic Socialists of America. (D S A)
Radical activist Noam Chomsky was also a member of the New Party.
The Democratic Socialists of America, are self described as the largest socialist organization in the United States and the principle U.S. affiliate of the Socialist International.
The New Party works alongside a group known as ACORN. As an organizer, Obama trains ACORN employees. As a lawyer, Obama represents ACORN in a lawsuit. ACORN has come under investigation in at least 14 states for voter registration fraud.
He meets the Rev. Jeremiah Wright, a former Muslim turned Christian. Wright's sermons are fiery anti-American, anti- white diatribes.
In Jeremiah Wright's most famous sermon, he says God bless America? No. No. No. God Damn America.
Obama calls Wright his "friend and mentor".
Obama's law firm represented a developer. He strikes a deal between his client and Lebanese businessman Tony Rezko to build low income housing. Rezko is known as a slum landlord and his housing projects are not well maintained. Rezko becomes an early Obama contributor. Obama buys a house with Rezko even while Rezko is under investigation in a corruption scandal. Rezko is found guilty on 16 of 24 charges.
Obama attends annual banquets of the Arab American Action Network (A.A.A.N.). He supports the Pakistanis. He confers with PLO adviser Edward Said. At the 2003 annual banquet of the A.A.A.N., he makes a toast to Chicago professor and former PLO Spokesman Rashid Khalidi.
He describes Israel's actions as "genocide" against the Palestinian people. Weather Underground Founders Bill Ayers and Bernadine Dohrn are in attendance.
In his bid for the presidency, Obama gets millions of dollars in illegal campaign contributions, many from foreign sources.
$33,000 came from the Rafah refugee camp in Gaza. Phone banks are set up in Gaza to solicit donations.
At least $500,000 is received from foreign sources not identified, and reported as being "not employed".
Obama is funded by George Soros, a billionaire and international socialist. Soros writes a book calling for an international government.
He also receives the support from the union's. He confers regularly with S.E.I.U. president Andy Stern. Stern has said " workers of the world unite, it's not just a slogan anymore".
As a United States Senator, Barack Obama was rated one of the most liberal. In 2007 he was rated the most liberal.
As president of United States, Barack Obama's actions have...
Threatened the U.S. Constitution.
Weakened America's defenses.
Encouraged our enemies.
Irritated our closest Allies.
Moved us toward Socialism.
Increased our budget deficit.
Increased our national debt.
Weakened our economy.
Trivialized the War on Terror.
Failed to meet his promises.
If you don't think it gets worse, think again. Neil Sankey and Susan Daniels comb through dozens of public databases and now allege that Obama has used multiple Social Security numbers during his life.
None of the social security numbers that Obama used were reissued by the state of Hawaii.
The social security number that Obama is now using ending in 4425 was issued in the state of Connecticut circa 1976 to 1979 to a person born in 1890.
If nothing else, this constitutes Social Security fraud and identity theft.
Here us the link to the Video
http://www.youtube.com/watch?v=eF58FmFAQvQ


Pet-Friendly Rental: How Do I Go About Finding One?
How Do I Find a Pet-Friendly Rental?
If you are a pet owner, it can be very difficult to find a pet-friendly rental in St. George and in many areas of Utah. This can be quite stressful when you have a pet and need to find a good home for the both of you. If you are in the situation of finding a rental space for yourself and your pet, make sure that you leave yourself enough time. Pet-friendly rentals are hard to come by, and you want to have at lease six weeks to look for a place and find the right fit.
A great resource for finding pet-friendly rentals is the Humane Society or the animal care or control shelter. Nonprofit places like this will often keep lists of pet-friend communities and rentals on hand, just for this purpose. Other websites with ads for rental properties will generally let you specify whether you are looking for a dog- or cat-friendly rental, so you can see options in your area quickly at a glance.
You may have to come to terms with the fact that your first, second, and even third choice of rental properties, just will not budge on a no-pet policy. Start off instead looking in condos, or privately owned rental units. Take note of who else has pets nearby the areas you check out, and see if they are well-behaved and well-cared for. You'll want to know that you are joining a community of responsible residents and pet-owners.
It is also great practice as a pet owner to gather documentation that you are a responsible tenant. Showing any training certificates that your dog has can really help. Have favorable references from past landlords that describe how your pet was well-behaved. Also in this situation, a letter from your vet showing that your pet is fully vaccinated and spayed or neutered can't hurt. It is good to show that you have been thorough and conscientious in your pets care.
Make sure you are willing as a pet owner to pay a little extra. Having a pet-friendly rental in St. George will often require a pet deposit and possible a monthly pet fee. Your willingness to pay may show your landlord that you do not have worries about the rental price or your income. Also, communicate to you potential landlord that pet-owners make great tenants. Pet-friendly rentals are hard to find, so you are interested in staying for a long time. Also let the landlord know that you are just as committed to your pet's behavior and the cleanliness of your home as he or she is. You are in this together, and you can be trusted to manage your pet and all responsibilities related to pet-ownership.


text:
Fritz Rimrott (ur. 20 września 1849 w Aschersleben, zm. 14 września 1923 w Wernigerode) – inżynier mechanik, konstruktor lokomotyw, menadzer kolejowy, m.in. prezes Dyrekcji Kolei w Gdańsku (1908-1920).

Życiorys
Po ukończeniu Szkoły Realnej w Aschersleben, uczęszczał do Szkoły Handlowej w Halberstadt a następnie studiował budowę maszyn na Królewskiej Akademii Przemysłowej w Berlinie (Königlichen Gewerbe-Akademie). Po jej ukończeniu podjął pracę na kolei. W 1875 zdał egzamin państwowy i uzyskał tytuł inżyniera mechanika (Maschinenbauführer) w służbie Prusko-Heskiego Zarządu Kolei Państwowych (Preußisch-Hessische Staatseisenbahnvervaltung). W 1881, w trakcie prac do drugiego egzaminu państwowego wynalazł jeden z typów lokomotywy parowej tzw. lokomotywę Rimrotta-Malleta (Rimrott-Mallet Locomotive), którą opracował wkrótce po Mallecie, jedenakże niezależnie od niego. W latach 1904-1906 był pracownikiem Dyrekcji Kolei w Berlinie (Eisenbahndirektion Berlin), następnie utworzonego zarządu kolei, gdzie zajmował się pracami projektowymi taboru jak i jego zakupem. Kilkakrotnie powierzano mu obowiązki prezesa kolejowych dyrekcji okręgowych - w Królewcu (Eisenbahndirektion Königsberg/Pr.) (1907-1908), i w Gdańsku (Eisenbahndirektion Danzig) (1908-1920), skąd w 1920 odszedł na emeryturę. Uhonorowano jego dorobek na Wyższej Szkole Technicznej w Gdańsku (Technischen Hochschule Danzig) nadając mu tytuł dr inż. h.c. (Dr.-Ing. E.h.). Od 1921 był członkiem zarządu Niemieckiego Towarzystwa Maszyn Technicznych (Deutsche Maschinentechnische Gesellschaft).

Bibliografia
 Udo Przygoda: Malletlok 13 des Frankfurter Feldbahnmuseums, Die Museums-Eisebahn 2/1998
 Rudolf Vierhaus (red.): Deutsche biographische Enzyklopädie, tom 8, Walter de Gruyter 2005, s. 423
 Über das Rahmen-Gelenk und den Rahmen von Mallet-Lokomotiven, Jan Hartmann Nürnberg 2015

Przypisy

Ludzie związani z kolejnictwem
Ludzie związani z Gdańskiem
Urodzeni w 1849
Zmarli w 1923


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How to accurately determine what stage of the market cycle you're in at any given time. Knowing this will allow you to adjust your buying and selling strategy. You won't just increase your profits...you'll turbo-charge them!
Dear Dave, I just wanted to share my experience with you since it has now been more than 12 months since I first started your training. I appreciate the opportunity and have enjoyed helping others learn and achieve some of the same successes I have been so blessed with.
Hey guys I want to write you about some good news. We were able to retire my Dad from the funeral business, permanently! This past November my Dad and I purchased a 108 unit multi family property in Dallas. My Dad has been in the funeral business for years. He was burned out talking to people about death all the time. He was able to leave his job this past January and now he's free as a bird! For myself, I was living in a hotel broke as a Texas joke just two years ago selling insurance. I am free too, thanks to you two. Thank you so much for everything you do! We now own over 350 commercial units and are growing each and every day. God Bless you!
Hi Dave! We just wanted to say thank you so very much for providing us with your experience and leadership. Your training has provided us with the tools we needed to negotiate, perform, finance, and close. We closed on a 16 unit property recently are closing on another 20 unit apartment next month. When some of us start out, the fact that we can own an apartment is daunting, if not impossible. But with all the education you supply us, the way to take action, and especially the "hope" you give us, we felt we could do this; Shari and I want to thank you so much for everything you do.
The security code on you credit or debit card is a three or four digit number. Cards issued by VISA®, MasterCard®, and Discover® have a three digit number located on the back of the card near the signature panel. American Express® cards have a four digit number on the front of the card that is generally located just above the account number.
PLEASE CHECK YOUR PROMO CODE AND TRY AGAIN!


John Wall, who had cleanup surgeries on both of his knees in May, has yet to play one-on-one yet as he continues his rehab.
Wall is going to take his time and he's certainly not going to set expectations in late-August because there's no reason for him to go there. If he's not healthy enough to go, the Wizards will have no problem sticking him on the bench and making sure he's healthy. We're nowhere near concluding that and this is a typical summertime non-update update.