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'PUPPET OF FRESHMAN': Pelosi Gets Blasted For Losing Control Of Party
@realsaavedra
House Speaker Nancy Pelosi has lost control of her party over Rep. Ilhan Omar's (D-CA) anti-Semitism scandal, according to numerous prominent pundits.
The Daily Wire reported that "on Wednesday, asked by a reporter about comments made by Rep. Ilhan Omar (D-MN) that have widely been interpreted as anti-Semitic, House Speaker Nancy Pelosi, who has assiduously avoided the idea of taking Omar off of the House Foreign Affairs Committee, answered that she did not think Omar's comments were 'intentionally anti-Semitic.'"
The Washington Examiner reported that Pelosi said that the House Foreign Affairs Committee, which Omar is a member of, would be writing the resolution.
Late on Wednesday, the Daily Beast reported that after pressure from far-left Democrats, "leaders appeared to change course, asking the House Foreign Affairs Committee to draft a resolution that rebuked 'all hate.'"
The apparent lack of control by Pelosi caught the attention of many notable pundits, relevant figures in media and politics, and notable social media accounts, who accused Pelosi of losing control to freshman.
John Podhoretz: "Congratulations to Nancy Pelosi, puppet of freshmen"
Congratulations to Nancy Pelosi, puppet of freshmen
— John Podhoretz (@jpodhoretz) March 7, 2019
Josh Jordan: "It's amazing to see someone as skilled and experienced as Pelosi get completely outmatched by a bunch of first term House reps who refuse to condemn antisemitism within the party."
It's amazing to see someone as skilled and experienced as Pelosi get completely outmatched by a bunch of first term House reps who refuse to condemn antisemitism within the party.
— Josh Jordan (@NumbersMuncher) March 7, 2019
Stephen Miller: "It took less than 3 months for Pelosi to lose control of her party. Just wild."
"Watching Pelosi deal with this is like watching Boehner & MConnell deal with Ted Cruz, except there are 4 of him and all 4 are raging anti-semites," Miller added. "She's lost the party."
It took less than 3 months for Pelosi to lose control of her party. Just wild.
— Stephen Miller (@redsteeze) March 7, 2019
Watching Pelosi deal with this is like watching Boehner & MConnell deal with Ted Cruz, except there are 4 of him and all 4 are raging anti-semites. She's lost the party.
Arthur Schwartz: "Pelosi seems to have lost control of her conference. Along with her spine."
Pelosi seems to have lost control of her conference. Along with her spine. https://t.co/SFwNVSAIh2
— Arthur Schwartz (@ArthurSchwartz) March 6, 2019
Ben Shapiro: "Pretty obvious who's running the party at this point, and it ain't Pelosi"
"Pelosi and company have decided to support the most anti-Semitic wing of the party in order to shore up a political coalition," Shapiro later added. "There is no principle here, just rank partisan interest."
Pretty obvious who's running the party at this point, and it ain't Pelosi https://t.co/BWmsfDgtWB
— Ben Shapiro (@benshapiro) March 6, 2019
Pelosi and company have decided to support the most anti-Semitic wing of the party in order to shore up a political coalition. There is no principle here, just rank partisan interest.
Former New York State Democrat Dov Hikind: "After getting pushed around by freshmen reps in the House, it's clear Pelosi is the leader in name only. And a feckless one at that. She couldn't even pass a toothless resolution condemning vile antisemitism. Shame on @SpeakerPelosi, @AOC, @IlhanMN and Shame on the Democrats!"
After getting pushed around by freshmen reps in the House, it's clear Pelosi is the leader in name only. And a feckless one at that.
She couldn't even pass a toothless resolution condemning vile antisemitism.
Shame on @SpeakerPelosi, @AOC, @IlhanMN and Shame on the Democrats! pic.twitter.com/94kjUkH5TI
— Dov Hikind (@HikindDov) March 7, 2019
Dana Loesch: "So with the failure to hold Omar accountable for her repeat anti-Semitic Tweet storms, Nancy Pelosi has shown she's lost control of the House — and her party. Meet the new Democrats/Socialists."
So with the failure to hold Omar accountable for her repeat anti-Semitic Tweet storms, Nancy Pelosi has shown she's lost control of the House — and her party. Meet the new Democrats/Socialists.
— Dana Loesch (@DLoesch) March 6, 2019
Fox News reported that "Pelosi is 'taken aback' by the growing dissent and anger among rank-and-file Democrats over a possible resolution to formally condemn anti-Semitism," according to a Democratic source, which highlighted "Pelosi's tenuous grip on control over the House and underscoring the growing power of the party's nascent far-left progressive wing."
Fox News added that "Pelosi even reportedly walked out of a meeting Wednesday with Democrat House members, setting down her microphone and telling attendees, 'Well if you're not going to listen to me, I'm done talking.'"
The Democratic source told Fox News: "Here we are again, fighting with ourselves. I've spent another week dealing with this and not on policy."
Read More: Anti-Semitism Ilhan Omar Nancy Pelosi


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Tag Archives: Water
Study: the early Earth's atmosphere contained oxygen
Christianity and the progress of science
Here's a paper published in the prestigious peer-reviewed science journal Nature, entitled "The oxidation state of Hadean magmas and implications for early Earth's atmosphere". This paper is significant because it undermines naturalistic scenarios for the origin of life.
Evolution News explains what the paper is about.
A recent Nature publication reports a new technique for measuring the oxygen levels in Earth's atmosphere some 4.4 billion years ago. The authors found that by studying cerium oxidation states in zircon, a compound formed from volcanic magma, they could ascertain the oxidation levels in the early earth. Their findings suggest that the early Earth's oxygen levels were very close to current levels.
[…]Miller and Urey conducted experiments to show that under certain atmospheric conditions and with the right kind of electrical charge, several amino acids could form from inorganic compounds such as methane, ammonia, and water. Several experiments have been done using various inorganic starting materials, all yielding a few amino acids; however, one key aspect of all of these experiments was the lack of oxygen.
If the atmosphere has oxygen (or other oxidants) in it, then it is an oxidizing atmosphere. If the atmosphere lacks oxygen, then it is either inert or a reducing atmosphere. Think of a metal that has been left outside, maybe a piece of iron. That metal will eventually rust. Rusting is the result of the metal being oxidized. With organic reactions, such as the ones that produce amino acids, it is very important that no oxygen be present, or it will quench the reaction. Scientists, therefore, concluded that the early Earth must have been a reducing environment when life first formed (or the building blocks of life first formed) because that was the best environment for producing amino acids. The atmosphere eventually accumulated oxygen, but life did not form in an oxidative environment.
The problem with this hypothesis is that it is based on the assumption that organic life must have formed from inorganic materials. That is why the early Earth must have been a reducing atmosphere. Research has been accumulating for more than thirty years, however, suggesting that the early Earth likely did have oxygen present.
[…]Their findings not only showed that oxygen was present in the early Earth atmosphere, something that has been shown in other studies, but that oxygen was present as early as 4.4 billion years ago. This takes the window of time available for life to have begun, by an origin-of-life scenario like the RNA-first world, and reduces it to an incredibly short amount of time. Several factors need to coincide in order for nucleotides or amino acids to form from purely naturalistic circumstances (chance and chemistry). The specific conditions required already made purely naturalist origin-of-life scenarios highly unlikely. Drastically reducing the amount of time available, adding that to the other conditions needing to be fulfilled, makes the RNA world hypothesis or a Miller-Urey-like synthesis of amino acids simply impossible.
So here's where we stand. If you are a materialist, then you need a reducing environment on the early Earth in order to get organic building blocks (amino acids) from inorganic materials. However, the production of these organic building blocks (amino acids) requires that the early Earth atmosphere be oxygen-free. And the problem with this new research, which confirms previous research, is that the early Earth contained huge amounts of oxygen – the same amount of oxygen as we have today. This is lethal to naturalistic scenarios for creating the building blocks of life on the Earth's surface.
Other problems
If you would like to read a helpful overview of the problems with a naturalistic scenario for the origin of life, check out this article by Casey Luskin.
The "origin of life" (OOL) is best described as the chemical and physical processes that brought into existence the first self-replicating molecule. It differs from the "evolution of life" because Darwinian evolution employs mutation and natural selection to change organisms, which requires reproduction. Since there was no reproduction before the first life, no "mutation – selection" mechanism was operating to build complexity. Hence, OOL theories cannot rely upon natural selection to increase complexity and must create the first life using only the laws of chemistry and physics.
There are so many problems with purely natural explanations for the chemical origin of life on earth that many scientists have already abandoned all hopes that life had a natural origin on earth. Skeptical scientists include Francis Crick (solved the 3-dimensional structure of DNA) and Fred Hoyle (famous British cosmologist and mathematician), who, in an attempt to retain their atheistic worldviews, then propose outrageously untestable cosmological models or easily falsifiable extra-terrestrial-origin-of-life / panspermia scenarios which still do not account for the natural origin of life. So drastic is the evidence that Scientific American editor John Horgan wrote, "[i]f I were a creationist, I would cease attacking the theory of evolution … and focus instead on the origin of life. This is by far the weakest strut of the chassis of modern biology."3
The article goes over the standard problems with naturalistic scenarios of the origin of life: wrong atmosphere, harmful UV radiation, interfering cross-reactions, oxygen levels, meteorite impacts, chirality, etc.
Most people who are talking about intelligent design at the origin of life talk about the information problem – how do you get the amino acids to form proteins and how do you get nucleotide bases to code for amino acids? But the starting point for solving the sequencing problem is the construction of the amino acids – there has to be a plausible naturalistic scenario to form them.
Amino AcidAmmoniaAtmosphereBlindBlockBoilingBuildingCarbonCellChemicalChiralityCompoundCredulityCrickDioxideDiscoveryDNAEarlyEarthEvidenceEvolutionExtinctionFaithGasGassesHydrogenKenyonLifeLivingMaterialismMeteoriteMethaneMolecularNaturalismOOLOparin-HaldaneOriginOxydizingOxygenOzonePrimordial SoupProductProgressProteinRadiationReactantReactionReasonReducingScienceSynthesizeTarThaxtonUltra-VioletUltravioletUVVaporWaterWatson
03/11/2016 Wintery Knight	5 Comments
Apologetics and the progress of science

redpajama_set_name: RedPajamaCommonCrawl


To etch or carve something into a surface or material. When we got our sidewalk repaved, the kids engraved their initials into the cement. The woman at the store said that they can engrave our wedding date into the picture frame.
1. To etch or carve something onto some surface or material. The woman at the store said that they can engrave our wedding date upon the picture frame.
2. By extension, to commit something to memory. After missing my first appointment, I engraved the rescheduled date upon my brain.
1. To etch or carve something onto a surface or material. The woman at the store said that they can engrave the picture frame with our wedding date.
2. To use something, such as a tool, to etch or carve into a surface or material. The artist engraved a design into the linoleum with a small cutter.
The research team said it hoped the engravings, formally known as petroglyphs, would help to provide a better understanding of its archaeological and ethnographic context.
The focus of GWs Radiance Glass is large format decorative glass products engraved with Radiances surface laser engraving technology from its German partner, Cerion Laser.
The researchers' analysis revealed that the marks were engraved intentionally, which suggests that these engravings were a purposeful component of a multi-stage cannibalistic ritual.
smartLEX offers perfect engraving of halftones or geometrical designs while keeping a very attractive TCO per engraved screen.
Founded in 1987, Rowmark is a manufacturer of extruded sheet materials servicing the engraving and custom decorative markets.
We have helped many electrical contractors find an in-house solution to their electrical engraving needs.
Another engraving was three goblets showing the Arms of Lady Jane Grey, husband Guilford Dudley and the Tudor Coat of Arms, featuring in a permanent exhibition at Bradgate Park, Leicestershire.
By contrast, the surface after engraving with a laser will have a matte finish.
7) Dunlap had already mentioned in his history Edwin's engraving of Edward Shippen (1729-1806), a chief justice of the Pennsylvania Supreme Court.
Mr Grenier, who lives in North Cadbury, Somerset, has been engraving for 20 years after training at West Dean College, Sussex, and then as a student of Simon Whistler, son of the famous glass engraver Lawrence Whistler.
The art of engraving is in a new renaissance period.
In celebration of its 30th anniversary of partnership with and promotion for the industry, Baron Engraving has prepared an exquisitely engraved Winchester Model 1892 Takedown as the 2012 SHOT Show rifle.
Following this, Sturm Ruger has had 1,000 of these pistols made with a special-edition slide engraved by Baron Engraving, which runs Ruger's Custom Engraving Shop.
US multi-industry manufacturer Standex International (NYSE:SXI) said on Thursday it had bought Indian mold textures specialist Melco Engraving India Private Limited (MEIPL), for an undisclosed sum.
The exhibition will present the entire collection, 100 pieces, considered the most important engraving series from the first half of the 20th century.


Using hand casting techniques, we are proud of our reputation for making beautifully finished beds that are designed and built to last forever.
Every bed has our unique cast knuckle joint to attach the side rails to the head and foot of the bed. This self locking system ensures a lifetime of service, and is incomparable to modern flat pack beds that are held together with often flimsy bolts. The range includes traditional iron, brass and nickel beds, day beds, four posters, half testers and headboards, and we also offer a host of bespoke options in addition to all the standard sizes.


It's about pondering larger, activating management in any respect levels, and driving innovation to create well being selling environments in the places we spend our time; from our colleges and workplaces, to sports golf equipment, marae and other key neighborhood settings. Board of Well being confirmed synthetic trans-fat regulation for City of Chelsea, creating a zero tolerance for partially hydrogenated elements in Chelsea's food service establishments. Healthy Chelsea's full-time College Coordinator continued as co-chair of faculty district's wellness committee. The USDA's Smart Snacks in Faculty diet requirements revealed final year are science-based mostly requirements for all meals and drinks sold to students in the course of the school day.
But that is what food firms have been calling wheat from which the germ and bran have been removed, leaving what is in effect pure starch, devoid of the fiber, oils, iron and nutritional vitamins that make wheat nutritious. Following the eight healthy consuming objectives above will help your body get the nutrients it needs. Select baked or grilled meals as a substitute of fried when you're eating out and implement this at dwelling, too.
This methodology seems to be better than some other as a result of it is quicker, requires minimum gear and the meals nonetheless tastes good and is as nutritious. The Healthy Land and Water Awards class winners, including the Individuals's Choice Award and Minister's Grand Prize, are introduced at a particular Gala Dinner on Friday 1 September 2017! Contemporary Meals Retail Improvement – Corner Store Conversions : This temporary appears to be like at methods to create healthier nook shops by means of modest infrastructural changes and retailer structure modifications.
Including garlic and onions is one other nice heart healthy option to drink your self into a healthier future. The cornerstone of a healthy food plan pattern needs to be to switch processed food with real food each time doable. In 2012, Healthy Chelsea continued its focus in Chelsea Public Colleges, with an added emphasis on School Lunch. There are some cravings that must be taken care of, however healthy alternatives will be discovered.
It is necessary to pay attention to what's in your food as producers usually conceal giant quantities of sugar or unhealthy fat in packaged food, even food claiming to be healthy. The whole concept of getting an simply digestible , healthy lunch is that the stomach could also be empty by tea-time to cater for the common cravings as per the mother-to-be's bio- clock So teatime, if hungry, a cup of lemon tea with some gingerbread or whole meal bread with honey could be a good idea.


Kona took the aggressive and dynamic geometry of the trail-happy Honzo and gave it a 27.5-inch-plus wheel size for those wanting to put more rubber to the trail.
Available SoonSorry, 'Kona 2018 Big Honzo DL Frame with SRAM Maxle Ultimate, XL' is currently out of stock. Please check back later or contact Bikeman for an expected availability date. Refer to our Shipping Terms for more information.


Today Nang is the day shift supervisor of the company's plastic manufacturing operations. Brandy is a product inspector for its AdvantaPure brand of molded silicone components. Josh Ream (pictured), a thirteen year employee, supervises the company's silicone tubing manufacturing team, and Monica Dann (also pictured; eight years) is a shift supervisor for silicone molding. The majority of NewAge's Cambodian team members are employed in the silicone extrusion and molding departments.


ISLAMABAD (92 News) – Former prime minister Nawaz Sharif has said that he has no quarrel with the judiciary, but has differences with some judges.
The PML-N president said that he had been punished and the accusation was being searched now.
"I cannot be intimidated. We are standing for the principle and the people are with me," he maintained.
Criticizing the judges, he said that the court had disrespected and sent home those serving the masses. "The court gave a certificate of being 'Sadiq' and 'Ameen' to a man who had admitted his assets," he said.
He presented a salute to the judges pronouncing the judgment.


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Home - Blog - Racial Equity and Racial Equality: What Do They Mean?
Racial Equity and Racial Equality: What Do They Mean?
by United Way NCA
Learn more about what racial equity means and other racial justice related terms. Including: What is the difference between racial equity and racial equality? Educate yourself about racial justice and get involved in empowering your community with United Way NCA.
What is the Difference between Racial Equity vs. Equality?
The pursuit of racial justice, like many social justice movements, can feel like facing a giant. However, despite the challenge, we can all do our part (big or small) to help make our communities more equitable and safer for everyone. One of the most crucial first steps to creating an equitable future is recognizing what it means, how it impacts you and your community, and your role in achieving it.
Although they are similar in a lot of ways, understanding the key differences between racial equity and equality is important to dismantling systemic racism and fostering a community that is inclusive for everyone. We're here to break down the differences between racial equity and racial equality, explaining why the difference matters and showing how United Way NCA is creating a more equitable future for the National Capital Area.
What is the Definition of Racial Equity?
Racial equity is achieved when race no longer factors into or determines one's socioeconomic outcomes. It is when everyone has what they need to thrive, no matter where they live or how they identify.
Working toward racial equity is one of the main pathways to achieving racial justice, which is the systematic fair treatment of people of all races that results in all people—regardless of their race, ethnicity or the community in which they live—having equal access to opportunities.
Though the ultimate goal of racial equity may be equality, the route to achieving equity cannot be accomplished simply through treating everyone equally. It is achieved by "treating everyone equitable, or justly according to their circumstances."
What is the Difference between Racial Equity and Racial Equality?
Equity is different from equality. Equality serves everyone the same, regardless of need. Equity, on the other hand, achieves fairness by meeting people where they are and serving them differently dependent on their needs to achieve equitable outcomes.
In relation to race, equity is achieved when all people—especially people of color that have historically been oppressed and marginalized—are the "owners, planners and decision-makers in the systems that govern their lives and are provided the infrastructure needed to thrive." Through racial equity, the needs of each community, group or individual are met and everyone benefits from a more just, equitable system.
What are Examples of Racial Equity?
Let's analyze a couple examples of what racial equity looks like:
1) A network of school systems has a goal for students to attain proficiency to conduct online research in their class. Some of the network's schools (A Schools) have a stronger IT infrastructure than others—greater bandwidth, more computers per student ratio, etc. Yet in the system's B Schools, like in far too many around the country, the IT infrastructure is least robust and advanced, leaving students at a disadvantage. The B Schools also disproportionately serve students of color compared to A Schools.
The school system has received a grant to improve middle school IT infrastructures. Funding is distributed according to each school's IT circumstances and the outcome is that students in B Schools now have the opportunity to perform along the same lines of students in A Schools, which they would not have had if funding had been distributed equally among the schools.
2) A city district has recently received funding designed to go toward infrastructure in their community and needs to decide on how to distribute resources. The southernmost parts of the district are predominantly middle-class white families and have recently undergone infrastructure developments on their main roads and parks. As you travel north, the neighborhoods are mainly lower-class racially and ethnically diverse families and have not had any major infrastructure development projects undertaken in their communities in over 10 years.
With equity in mind, the city district's leaders conclude that most of the funding should go toward proposed infrastructure development projects for northern neighborhoods that haven't had access to updates in over a decade, while the southern communities receive less than half of the funding because they recently underwent updates to their infrastructure and do not need extra funding to achieve the same infrastructure goals.
What is the Definition of Racial Equality?
Racial equality is serving everyone the same, no matter what their needs may be. While this may be the ultimate goal, it runs the risk of impeding the effort to close opportunity gaps and dismantling racial inequities when trying to achieve racial justice, because it does not take into consideration disparities in opportunities and resources across different communities. Racial equality can actually make inequities worse.
What are Examples of Racial Equality?
Taking the examples we shared above, let's analyze them as scenarios where equality is the focus:
1) If the school system had opted for equal funding per school, the resource access between schools would remain disproportionate, racial gaps would remain and existing racial inequities would not be addressed because the A Schools already had greater IT resources than the B Schools before extra funding was provided.
2) If the city's leaders chose to distribute resources equally between its neighborhoods and communities, those that historically haven't had equal access to infrastructure upgrades would continue to be behind those who have consistent access to project funds. Therefore, the gaps and existing inequities between the white, middle-class neighborhoods and diverse, lower-class ones would remain and even become more disproportionate.
How is United Way NCA Improving Racial Equity?
United Way of the National Capital Area believes everyone deserves hope, respect and a fair chance. That's why we're creating a more equitable future for all community members by improving the region's health, education and economic opportunity.
Our health programs increase equity in access to health resources that promote physical and mental wellbeing among students and families. We also work to reduce academic disparities and improve academic outcomes for young people in the National Capital Area by focusing on the education pipeline from middle school to college and/or career success. Finally, United Way NCA seeks to provide residents with economic opportunity and removing barriers to stable and affordable housing.
How Can You Practice and Promote Racial Equity and Equality in Your Community?
If you're feeling discouraged, we're here to tell you that you can take actionable steps right now to help practice and promote equity in your community, household, workplace, place of worship and other spheres of influence you are a part of.
Reflect on your own belief system. What implicit biases do you hold? How can you dismantle them? How can you educate yourself through books, media, diversity and inclusion seminars, etc. to understand equity further? Sign up for our 21 Day Race Equity Journey, a 21-day newsletter series, to learn more about unpacking how equity plays a role in determining outcomes of people through different stages of life depending on their intersections of race, gender, sexuality and/or socioeconomic standing.
Get involved! Reaching an equitable future for all community members necessitates action. By supporting nonprofits and programs like United Way NCA, you can make a difference. This can be done through monetary donations, corporate sponsorships of programs, volunteering, advocating and more.
This fall, United Way NCA will launch our Practice Equity campaign, in which we will share how community members can practice equity daily. Follow us on Facebook, Twitter, Instagram and LinkedIn to stay tuned.
Learn more about equity and how United Way NCA is achieving a more equitable future by visiting unitedwaynca.org/equity and join the movement!
When none are ignored, all will thrive.
About United Way of the National Capital Area
United Way of the National Capital Area improves the health, education and economic opportunity of every person in the National Capital community. United Way NCA has been improving lives by creating measurable impact in the District of Columbia, Northern Virginia, and Montgomery and Prince George's counties for more than 45 years. In 2020, United Way NCA was among 384 organizations across the United States to receive a generous transformational investmentfrom novelist and venture philanthropist, MacKenzie Scott. For more information about United Way of the National Capital Area, visit UnitedWayNCA.org.
Vacant Homes vs. Homelessness in Cities Around the U.S.
For many Americans, finding affordable housing continues to be a challenge, whether you're renting or buying. In today's real estate market, many overpriced homes sit vacant while populations experiencing homelessness […]
Highest Graduation Rates by State & Metro Counties
At United Way, we see firsthand how much a quality education can have a major lifelong effect on the lives of children in their communities. That's one of many reasons […]
Diversity and Inclusion Training: Everything You Need to Know
In today's workplace, diversity and inclusion training programs are more important than ever. By cultivating a more diverse and inclusive workplace, your company can embrace people from all walks of […]
Stay Connected to United Way NCA
Our quarterly newsletter, Community Matters, keeps you informed on all things United Way NCA, including volunteer opportunities, news, upcoming events to attend, a letter from our president & CEO, Rosie Allen-Herring, and so much more.


SKU: 970-5B. Categories: Biopsy Kits, Specimen Collection.
Multi-compartment biopsy containers available with or without pre-filled 10% formalin.
Dimensions of all CoreDish® containers are: 1 1/16″ deep x 3 3/4″ in diameter, with a 1 1/8″ label area.


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Q: Can't Load my Assets when running my java AWT game jar by RightClicking on MacOS i made a game with awt and made a jar out of it . but when i run it by right clicking it it doesnt load the assets ( assets are on the jar file) But then i run it with terminal it loads the assets !
i'm using MacOS Monterey and Java 17
i used this code to get a image :
import java.awt.*;
import java.awt.image.BufferedImage;
import java.io.File;
import java.io.IOException;

public class Image {
    public BufferedImage image;
    public Image(String Path){
        BufferedImage img = null;
        try {
            img = ImageIO.read(new File(Path));
        } catch (IOException e) {
        }

        this.image = img;
    }
    public static void drawImage(Graphics2D g,Image image,int x,int y,int w,int h){
        g.drawImage(image.image,x,y,w,h,null);
    }
}

and i called them like this:
Image image = new Image("Data/image.PNG");

// And in my draw Method:
public void draw(Graphics2D g){
        Image.drawImage(g,image,0,0,32,32);

}

the game with double clicking the jar on mac
game with double clicking(img)
and the game with opening the game with : (java -jar game.jar)
game with running on terminal(img)

redpajama_set_name: RedPajamaStackExchange


text:
Mobile |
Call of Duty: Mobile is a free-to-play first-person shooter game developed by TiMi Studios and published by Activision for Android and iOS It was released globally on October 1, 2019. It was originally announced in March of 2019. The closed beta was soon released in Australia and Canada. It features two in-game currencies, as well as a battle pass.The game received over 35 million downloads within three days of its release, earning over US$2 million in revenue. After one week, the game had surpassed 100 million downloads and generated over US$18 million in revenue, making it the largest mobile game launch in history. Source - Wikipedia
Call of Duty: Mobile is a free-to-play first-person shooter game developed by TiMi Studios and published by Activision for Android and iOS It was released globally on October 1, 2019. It was originally announced in March of 2019. The closed beta was soon released in Australia and Canada. It features two in-game currencies, as well as a battle pass.The game received ov
Babu R
Vihitharadhya R R
amazing graphics but they should improve battle royale


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Sen. Bob Casey urges lawmakers to give gun control measures thoughtful review and not hasty judgment
Updated Jan 05, 2019; Posted Jan 16, 2013
By Ivey DeJesus | idejesus@pennlive.com
U.S. Sen. Bob Casey, D-Pa.
U.S. Sen. Bob Casey, D-Pa., chairman of the Joint Economic Committee, makes his opening remarks Dec. 6 on Capitol Hill in Washington during a hearing on the 'fiscal cliff.'
(Photo by AP Photo)
Just hours after President Barack Obama unveiled a comprehensive plan to limit access to guns and address gun violence, Sen. Bob Casey, D-Pa., urged fellow lawmakers to give the measures thoughtful consideration and resist hasty judgment.
"I think whether as member of Congress or citizens we should examine closely and if we disagree we should make it known," Casey said. "But for politicians to start condemming when all they have read is the summary... I think people should, especially politicians, they aren't expressing opinion. They have to cast a vote. There should be some considered judgment, some thorough review before you make a blanket statement and say you are against it."
Casey appeared at a press conference in York just hours after the president signed 23 executive actions on gun control.
While his measures require no Congressional action, Obama also asked Congress to pass gun-control laws, including measures that would require background checks on all gun sales; re-instate a ban on "military-style assault weapons"; ban gun magazines with capacities of more than 10 rounds; and toughen certain penalties.
Casey said he would support the measures outlined by Obama.
"I hope it doesn't become a typical partisan fight in Washington," he said. "It should be a moment to come together in a common sense way."
He said no one was "under any illusion" that the measures would totally erase violence.
"This will take a generation to fix," Casey said.
Casey in recent weeks has come under attack from gun rights groups for coming out in support of a restoration of ban on assault weapons and high-capacity magazine clip weapons. Casey has particularly come under attack from the National Rifle Association, which long had given the second-term senator high marks on his gun-rights voting record.
Casey said he was used to being criticized, and recognized that the issue stimulated a lot of "emotion and at times anger."
"That's OK as long as we have a constructive debate," he said. "We have to try to do something here. We can't shrug our shoulders say it's too tough....I just think we've got to take some steps. And I think these steps are not only common sense but also don't infringe on the right of someone to hunt."
Casey said Pennsylvania's hunting tradition should "be honored and respected."
Casey said he was trying to show patience for people who disagreed with him but hoped that they would "sit back and think about this."
Flanked by City of York officials, including Chief of Police Wes Kahley, Casey outlined efforts he will push through the federal level to enhance law enforcement at the local level.
He called for increased funding for the so-called Cops Program, a competitive, grants-based hiring program that has put 55 police officers in York alone over the past couple of years. Casey said the program, authorized at up to $1 billion, was woefully underfunded.
Casey said he would also lobby for increased funding for a justice grant program that enhances law enforcement at the prosecution and court level, and funding for bullet-proof vests for police.
"I would like to find someone in Washington who can tell me why $6 million was cut from that program," Casey said. "What did that cut do to our economy? Of course the answer is not a bit. It's time for those who preach about law enforcement and how tough on crime they are and then vote for massive cutting on programs to explain that."


text:
"""
    Knowledge base module URLs
"""
from django.conf.urls.defaults import *

urlpatterns = patterns('maker.knowledge.views',
        url(r'^(\.(?P<response_format>\w+))?$', 'index', name='knowledge'),
        url(r'^index(\.(?P<response_format>\w+))?$', 'index', name='knowledge_index'),
        url(r'^categories(\.(?P<response_format>\w+))?/?$', 'index_categories', name='knowledge_categories'),

        # Folders
        url(r'^folder/add(\.(?P<response_format>\w+))?/?$', 'folder_add', name='knowledge_folder_add'),
        url(r'^folder/add/(?P<folderPath>.(?:[a-z,0-9,-]+/)+)(\.(?P<response_format>\w+))?/?$',
            'folder_add_folder', name='knowledge_folder_add_folder'),
        url(r'^folder/(?P<folderPath>.(?:[a-z,0-9,-]+/)+)(\.(?P<response_format>\w+))?/?$',
            'folder_view', name='knowledge_folder_view'),
        url(r'^folder/edit/(?P<knowledgeType_id>\d+)(\.(?P<response_format>\w+))?/?$',
            'folder_edit', name='knowledge_folder_edit'),
        url(r'^folder/delete/(?P<knowledgeType_id>\d+)(\.(?P<response_format>\w+))?/?$',
            'folder_delete', name='knowledge_folder_delete'),

        # Knowledge Items
        url(r'^item/add(\.(?P<response_format>\w+))?/?$', 'item_add', name='knowledge_item_add'),
        url(r'^item/add/(?P<folderPath>.(?:[a-z,0-9,-]+/)+)(\.(?P<response_format>\w+))?/?$',
            'item_add_folder', name='knowledge_item_add_folder'),
        url(r'^(?P<folderPath>.(?:[a-z,0-9,-]+/)+)(?P<itemPath>.(?:[a-z,0-9,-]+/)+)(\.(?P<response_format>\w+))?/?$',
            'item_view', name='knowledge_item_view'),
        url(r'^item/edit/(?P<knowledgeItem_id>\d+)(\.(?P<response_format>\w+))?/?$',
            'item_edit', name='knowledge_item_edit'),
        url(r'^item/delete/(?P<knowledgeItem_id>\d+)(\.(?P<response_format>\w+))?/?$',
            'item_delete', name='knowledge_item_delete'),

        # Categories
        url(r'^category/add(\.(?P<response_format>\w+))?/?$',
            'category_add', name='knowledge_category_add'),
        url(r'^(?P<categoryPath>.(?:[a-z,0-9,-]+/)+)(\.(?P<response_format>\w+))?/?$',
            'category_view', name='knowledge_category_view'),
        url(r'^category/edit/(?P<knowledgeCategory_id>\d+)(\.(?P<response_format>\w+))?/?$',
            'category_edit', name='knowledge_category_edit'),
        url(r'^category/delete/(?P<knowledgeCategory_id>\d+)(\.(?P<response_format>\w+))?/?$',
            'category_delete', name='knowledge_category_delete'),
)

redpajama_set_name: RedPajamaGithub


text:
package com.mesosphere.dcos.cassandra.common.offer;

import org.apache.mesos.Protos;
import org.apache.mesos.Protos.ExecutorInfo;
import org.apache.mesos.offer.InvalidRequirementException;
import org.apache.mesos.offer.OfferRequirement;
import org.slf4j.Logger;
import org.slf4j.LoggerFactory;

import java.util.Arrays;
import java.util.Optional;

public class ClusterTaskOfferRequirementProvider implements CassandraOfferRequirementProvider {
    private static final Logger LOGGER = LoggerFactory.getLogger(
            ClusterTaskOfferRequirementProvider.class);

    @Override
    public OfferRequirement getNewOfferRequirement(String type, Protos.TaskInfo taskInfo) {
        LOGGER.info("Getting new offer requirement for nodeId: {}",
                taskInfo.getTaskId());
        return getCreateOfferRequirement(type, taskInfo);
    }

    private OfferRequirement getCreateOfferRequirement(String type, Protos.TaskInfo taskInfo) {
        ExecutorInfo execInfo = taskInfo.getExecutor();
        taskInfo = Protos.TaskInfo.newBuilder(taskInfo).clearExecutor().build();

        try {
            return OfferRequirement.create(type, Arrays.asList(taskInfo), Optional.of(execInfo));
        } catch (InvalidRequirementException e) {
            LOGGER.error("Failed to construct OfferRequirement with Exception: ", e);
            return null;
        }
    }

    @Override
    public OfferRequirement getReplacementOfferRequirement(String type, Protos.TaskInfo taskInfo) {
        LOGGER.info("Getting replacement requirement for task: {}",
                taskInfo.getTaskId().getValue());

        ExecutorInfo execInfo = taskInfo.getExecutor();
        taskInfo = Protos.TaskInfo.newBuilder(taskInfo).clearExecutor().build();

        try {
            return OfferRequirement.create(type, Arrays.asList(taskInfo), Optional.of(execInfo));
        } catch (InvalidRequirementException e) {
            LOGGER.error("Failed to construct OfferRequirement with Exception: ", e);
            return null;
        }

    }

    @Override
    public OfferRequirement getUpdateOfferRequirement(String type, Protos.TaskInfo taskInfo) {
        return getExistingOfferRequirement(type, taskInfo);
    }

    private OfferRequirement getExistingOfferRequirement(String type, Protos.TaskInfo taskInfo) {
        LOGGER.info("Getting existing OfferRequirement for task: {}", taskInfo);

        ExecutorInfo execInfo = taskInfo.getExecutor();
        taskInfo = Protos.TaskInfo.newBuilder(taskInfo).clearExecutor().build();

        try {
            return OfferRequirement.create(type, Arrays.asList(taskInfo), Optional.of(execInfo));
        } catch (InvalidRequirementException e) {
            LOGGER.error("Failed to construct OfferRequirement with Exception: ", e);
            return null;
        }
    }
}


GOMEXUS Power Knob 35mm has direct fitment for several Shimano fishing reels.
Super light: 26g/0.92oz, 34.5mm/1.35″ in diameter.
The knob perfectly fits the Stella 5000FA handle, using the spare bearings and spacers came with the order. Quality is amazing for the price. In case, i will buy again for sure from this shop!
Looks really good on my penn conflict 2.


text:
Albert Duchêne est un footballeur français né le  à Aubevoye (Eure). Il a évolué comme gardien de but à Rouen, Metz et Reims.

Carrière de joueur
 1961-1969 : FC Rouen
 1969-1971 : FC Metz
 1971-1973 : Stade de Reims

Statistiques
  231 matchs en Division 1
  35 matchs en Division 2
  2 matchs en Coupe des villes de foires

Notes et références

Liens externes

Gardien de but français de football
Gardien de but du Football Club de Metz
Gardien de but du Stade de Reims
Gardien de but du Football Club de Rouen
Naissance en juin 1940
Naissance dans l'Eure

redpajama_set_name: RedPajamaWikipedia


text:
Q: Google Hacked IP Address - Subpoena to Google I suspected somebody hacked into my email account and sent messages from it, so I served Google with a subpoena to produce the IP addresses of the computer that sent the hacked emails.
Google produced the following:
X-Originating-IP: 2001:e68:5413:720c:885d:5a28:4583:a4ac

X-Originating-IP: 2001:e68:5413:720c:d45b:e46:2578:6ec9

X-Originating-IP: 2001:e68:5413:720c:3c4c:924d:f3bb:ffa1

Anyone know how to interpret this????

A: There are IPv6 IP adresses. The difference between familiar to you IPv4 adresses is that IPV6 one are 128 bits long.
All of them are located in Malysia so if you're not located there then it's likely you've been hacked.


I have been a reviewer for What's Good To Do for a couple of years now and we have had some great products to review and been on some amazing days out. Today we visited the Cold War Bunker at York and are looking forward to a trip to Frankie & Benny's next week as well as seeing The Lancashire Hotpots and An Evening of Poetry with Mike Harding at the Lowry in May.
What's Good to Do have entered the Virgin Media Business #Pitchtorich #VOOM 2015 competition and are currently in 85th place. They need to be in the top 50 before 5pm on Tuesday 5th May so please will you take a minute to vote for them.


text:
The following is the complete list of the 291 Virtual Console titles that have been released for the Nintendo 3DS in Japan sorted by system and release dates. English translations are highlighted between parentheses.

Available titles
The following is the complete list of the 279 Virtual Console titles available for purchase for the Nintendo 3DS in Japan sorted by system and release dates.

Game Boy
There are 70 games available to purchase.

Game Boy Color
There are 22 games available to purchase.

Game Gear
There are 22 games available to purchase.

Famicom
There are 97 Famicom games and 14 Disk System games available to purchase.

Super Famicom
There are 49 games available to purchase on the New Nintendo 3DS platforms (New Nintendo 3DS, New Nintendo 3DS LL and New Nintendo 2DS LL).

PC Engine
There are 3 games available to purchase.

Delisted titles
There are 4 games that were previously available for purchase but are not anymore.

Game Boy

Game Boy Color

PC Engine

Promotion-exclusive titles
The following is the complete list of the 13 Virtual Console titles which were available for the Nintendo 3DS in Japan exclusively by special promotion, sorted by system and release dates.

Famicom
There is 1 game which was promotion-exclusive.

Game Boy Color
There are 2 games which were promotion-exclusive.

Game Boy Advance
There are 10 games which were promotion-exclusive. These are the 10 Game Boy Advance games that were available exclusively for Nintendo 3DS Ambassadors.

See also
List of Virtual Console games for Wii (Japan)
List of Virtual Console games for Wii U (Japan)
List of DSiWare games and applications
3D Classics

References

Video game lists by platform
Nintendo-related lists


text:
Olive Mary Hilliard ( Hillary, 4 July 1925 – 30 November 2022) was a South African botanist and taxonomist. Hilliard authored 372 land plant species names, the fifth-highest number of such names authored by any female scientist.

Hilliard was born in Durban on 4 July 1925. She attended Natal University from 1943 to 1947, where she obtained an MSc and later a PhD. She worked at the National Herbarium in Pretoria in 1947-48 and was a lecturer in botany at Natal University from 1954 to 1962. In 1963 she became curator of the herbarium at Natal University and a research fellow. Her special fields of interest were the flora of Natal and the taxonomy of Streptocarpus, Compositae and Scrophulariaceae.

In 1964 she formed a professional and personal collaboration with Brian Laurence Burtt (1913-2008) who played a large part in the revitalising of a moribund Royal Botanic Garden Edinburgh. Their collaboration resulted in numerous papers and three books, Streptocarpus: an African Plant Study (1971), The Botany of the Southern Natal Drakensberg (1987), and Dierama: The Hairbells of Africa (1991).

Hilliard died on 30 November 2022, at the age of 97.

Legacy
Hilliard collected specimens, mostly from the Natal Drakensberg and Malawi, number some 8000 (of which 5000 were collected with B. L. Burtt). She is commemorated in the 2 genera of Hilliardia and Hilliardiella (both in the Asteraceae family). She is also honoured in Plectranthus hilliardiae , Schizoglossum hilliardiae , Cymbopappus hilliardiae , Agalmyla hilliardiae  and Helichrysum hilliardiae

Works
 Hilliard, OM, BL Burtt 1971. Streptocarpus: an African Plant Study
 Hilliard, OM. 1983. Flora of Southern Africa Series. Ed. Balogh Scientific Books. 325 pp.
 Hilliard, OM, BL Burtt 1985. A Revision of Geranium in Africa south of the Limpopo. (Notes from the Royal Botanic Garden Edinburgh. Vol. XLII no. 2)
 Hilliard, OM. 1987. The Botany of the Southern Natal Drakensberg (Annals of Kirstenbosch Botanic Gardens) Ed. National Botanic Gardens. 253 pp.
 Hilliard, OM, BL Burtt 1991. Dierama: The Hairbells of Africa. Ed. Timber Press, Inc. 152 pp.
 Hilliard, OM. 1995. The Manuleae: A Tribe of Scrophulariaceae. Ed. Edinburgh University Press. 600 pp.
 Hilliard, OM, LS Davis (illustrator). 1997. Trees & Shrubs of Natal (Ukhahlamba). Ed. Univ. of Kwazulu Natal Press; 2ª ed. 48 pp.
 Hilliard, OM. 1997. Flowers of the Natal Drakensberg: The Lily, Iris And Orchid Family And Their Allies (Ukhahlamba S.) Ed. Univ. of Kwazulu Natal Press. 85 pp.

References

1925 births
2022 deaths
20th-century South African botanists
20th-century South African women scientists
Botanists with author abbreviations
South African taxonomists
South African women botanists
Women taxonomists


Abstract: The combination of a prime mover and an energy storage device for reduction of fuel consumption has successfully been used in automotive industry. The shipping industry has utilised this for conventional submarines. The potential of a load levelling strategy through use of a hybrid battery–diesel–electric propulsion system is investigated. The goal is to reduce exhaust gas emissions by reducing fuel oil consumption through consideration of a re-engineered ship propulsion system. This work is based on operational data for a shipping fleet containing all types of bulk carriers. The engine loading and the energy requirements are calculated, and sizing of suitable propulsion and the battery storage system are proposed. The changes in overall emissions are estimated and the potential for fuel savings identified. The efficiency of the system depends on the storage medium type, the availability of energy and the displacement characteristics of the examined vessels. These results for the global fleet indicate that savings depending on storage system, vessel condition and vessel type could be up to 0.32 million tonnes in NOx, 0.07 million tonnes in SOx and 4.1 million tonnes in CO2. These represent a maximum 14% of reduction in dry bulk sector and 1.8% of world's fleet emissions.
► Global shipping makes a significant contribution to CO2, SOx and NOx emissions.
► We examine noon reports from a fleet of bulk carriers to identify the amount engine is operating off design.
► A hybrid propulsion system is proposed that uses multiple diesel–electric generators and battery storage.
► Analysis indicates hybrid may give an attractive rate of return as well as emissions savings in emissions.
► Implementation will require review of class society regulations.
Approximately 80% of world trade by volume is carried by sea (UNCTAD, 2008). In 2007 it is estimated that international shipping was responsible for approximately 870 million tonnes of CO2 emissions, or 2.7% of global anthropogenic CO2 emissions (IMO, 2009). Domestic shipping and fishing activity bring these totals to 1,050 million tonnes of CO2, or 3.3% of global anthropogenic CO2 emissions. Despite the undoubted CO2 efficiency of shipping in terms of grammes of CO2 emitted per tonne-km, it is recognised within the maritime sector that reductions in these totals must be made (IMO, 2009). Shipping is responsible for a greater percentage share of NOx (∼37%) and SOx (∼28%) emissions (AEA Energy & Environment, 2008) and recent legislation is aimed at reducing these emissions through the introduction of emission control areas and requirements on newly built marine diesel engines (MARPOL, 2005).
Costs per kilowatt hour for batteries range from $90 for lead acid to $110 for Sodium/nickel chloride to $300 for Vanadium–Bromine to $600 for Lithium Ion.
The principal disadvantage of Lithium Ion batteries in this application is their large cost which exceeds 600$/kWh. Lead acid batteries appear to be a more economic solution. However, the low material resistance in the marine environment, corrosive failures and the short life period of 400 complete charges and discharges, make them more expensive in the life cycle of the ship. Lead acid batteries suffer from a quick voltage drop and in a long period of storage from self-discharging.
The main engine cost is approximately 250 $/kW. However, the typical cost of diesel generator engines is significantly higher than the main engine. A typical price per kW of diesel generators is 350 $/kW (Fragkopoulos, 2007). Although the initial cost of such engines is higher, the advantage of prefabrication and the modular application of the machinery components, leads to saving in construction man-hours in shortening the whole construction time of the vessel. Thus, potentially the total construction costs are reduced (Gertsos et al., 2006) although this is not investigated further here. Furthermore, cost difference exists due to the installation of electric motors, cabling and other components of the electrical installation. An overall 6% increase in machinery cost will be assumed as the cost of the electrical components. The machinery cost is taken to be 30% of the total cost of the ship (Papanikolaou, 1994). Thus the extra machinery cost represents a 2% increase in the overall price of the vessel. The market value of the vessels is taken according to the current market state (Cotzias Shipping Group, 2010). Concerning the fuel price market, an average value for the year is taken equal to 520 $/tonne (Petromedia LTD, n.d.). However, the trend of fuel prices shows that its price is likely to be increased in future years. As a result, a rate of price increase of 10% each year is assumed. It is further assumed that after 25 years, the storage system can be sold for 10% of the original cost.
The value is >100% because in Handysize, Panamax, Post-Panamax, the payback period is 8, 19, 3 and 1 years, respectively, instead of 25 in other cases.
The study has shown that installing hybrid power technology on-board dry bulk ships can save fuel up to 1.27 million USD (at the price of 520$/tonne) per vessel and per year, assuming that the 60% of the time ship sails in laden and 40% in ballast condition. This value depends as well on the ship's dimensions, the storage medium adopted and the demand for energy availability. The emission reduction is achieved primarily through reducing the consumption of fuel and further reductions could be achieved by optimisation of the combustion process or the operation of other engine components. The combination of a hybrid energy storage and the flexibility that offers in the coupling with the propulsor, along with other possible improvements in hydrodynamics based improvement in ship energy efficiency should allow a step improvement in overall efficiency of ship propulsion systems (estimated between 2% and 10%) although this requires further systematic design studies.


text:
\section{Introduction}

Gravitational lensing has emerged as a powerful cosmological tool. The spectacular images provided by strong
lensing~\cite{1996ApJ...471..643K,Kneib:2001qy,Bradac:2006er} together with the robust parameter determination anticipated with weak lensing~\cite{Kaiser:1991qi,Mellier:1998pk,Bartelmann:1999yn,Hu:1999ek,Huterer:2001yu,Abazajian:2002ck,Takada:2003ef,Refregier:2003xe} are just two of
the exciting developments in the field. When astronomers look for lensing, they have demonstrated that they can
find it. Lensing can also contaminate observations of correlation functions because the images of objects are displaced from the true source positions. For example, it has long been known that lensing
smoothes out the spectrum of the cosmic microwave background (CMB)~\cite{Seljak:1995ve,Lewis:2006fu,Smith:2007rg}. The effect of lensing on galaxy-galaxy correlations
has been re-examined by several groups recently~\cite{Moessner:1997vm,Matsubara2000,Hui:2007cu,Vallinotto:2007mf,LoVerde:2007ke,Hui:2007tm,Schmidt:2008mb}. And a number of groups are anticipating the importance of lensing on future observations of neutral hydrogen via long wavelength measurements of the redshifted 21 cm line~\cite{Mandel:2005xh,Zhang:2006fc,Lewis:2007kz}.

In this work we present a unified treatment of the lensing contamination of correlation functions. First, we show that weak lensing contaminates \textit{any} cosmological correlation function. Whereas previous studies have quantified its effect on some specific correlation functions (for instance, CMB temperature and polarization \cite{Lewis:2006fu} and baryon oscillations through the galaxy correlation function \cite{Vallinotto:2007mf}), we focus here on the \textit{generality} of the result. This general framework allows us to understand when and for what correlation functions weak lensing represents a sizeable or a negligible effect. By working in real space, we also hope to provide physical intuition for some of the properties of the lensing effects, which is harder to obtain from a pure $k$-space calculation.
Second, we consider the dependence of the lensing effect on the orientation
of the source separation with respect to the line of sight. We also include the
lensing-induced time delay as the
longitudinal companion effect to the transverse lensing deflections.
Finally, we show how the general framework presented here can be applied to different correlation functions: we retrieve previous results for the CMB, supplement and correct previous galaxy-galaxy results~\cite{Vallinotto:2007mf}, and apply the formalism to the anisotropy induced by lensing of 21-cm radiation.

The paper is organized as follows. In Sec.~\ref{Sec:GenRes3D} a general formalism to calculate the weak lensing contribution to cosmological correlations is introduced along with a more physical understanding of the different quantities involved. In Sec.~\ref{Sec:Apps} the general formalism developed is applied to three different cases: correlation of galaxies, of the cosmic microwave background and of the 21-cm radiation. Finally, Sec.~\ref{Sec:Conclusions} contains some discussion together with concluding remarks. The calculations are relegated to the appendices.

\section{General Formalism}
\label{Sec:GenRes3D}

Weak lensing, i.e. the effect of small potential differences in the intervening space
on the path of light, consists to first order of two effects: a {\it transverse
deflection} of the photons from a straight path, and a {\it time delay} (Shapiro
delay) along the path. Together, these effects result in a three-dimensional displacement of the apparent source position.

Consider two physical observables $A(\vec{x}_a)$ and $B(\vec{x}_b)$ and denote the \textit{observed} values of $A$ and $B$ as $\tilde{A}(\vec{x}'_a)$ and $\tilde{B}(\vec{x}'_b)$. In this section we keep the nature of these cosmological observables \textit{completely unspecified}. The form of the results depends neither on the actual physical observables that are being correlated nor on the nature of the source of the signal that is used to measure them.
Since the geodesics light travels on are perturbed by the intervening distribution of
matter, the measured values of the observables refer to physical points that
are displaced with respect to the observed ones.

\begin{figure}[t]
\includegraphics[width=0.5\columnwidth]{deflection.eps}
\caption{Gravitational lensing bends photon trajectories. The sources, physically located at $\vec{x}_a$ and $\vec{x}_b$ are observed at $\vec{x}_a+\vec{\zeta}_a$ and $\vec{x}_b+\vec{\zeta}_b$ (in direction $\hat{n}_a$ and $\hat{n}_b$). $\alpha$ denotes the angle with the line of sight of the observed separation vector, $\vec{r}_{obs}$. \label{fig:deflection_geometry}}
\end{figure}

Consider the arrangement depicted in Fig.~\ref{fig:deflection_geometry}. Since
gravitational lensing perturbs the photons' trajectories, the two sources --
located at $\vec{x}_a$ and $\vec{x}_b$ -- are observed at
$\vec{x}'_a=\vec{x}_a+\vec{\zeta}_a$ and $\vec{x}'_b=\vec{x}_b+\vec{\zeta}_b$.
The observed distance
$\vec{r}_{\textrm{obs}}$ between the sources will in general differ from the
true distance $\vec{r}$. Whereas isotropy demands that the unlensed correlation
function depends only on the distance $r$, the lensed correlation function
depends on the angle $\alpha$ that $\vec{r}$ makes with the line of sight.
Note that any difference in the line-of-sight angle of $\vec{r}$ and
$\vec{r}_{obs}$ is a higher order correction, and we hence consider them to be
equal for the perturbative approach adopted in this paper.
Whenever the correlation function of two cosmological observables is measured,
such measurement is subject to a modification arising because of the
displacement of the apparent source positions $\vec{x}'_a$, $\vec{x}'_b$:
\begin{equation}\label{GenRes:xcorr1}
\langle \tilde{A}(\vec{x}'_a) \tilde{B}(\vec{x}'_b)\rangle=\langle A(\vec{x}'_a-\vec{\zeta}_a) B(\vec{x}'_b-\vec{\zeta}_b)\rangle.
\end{equation}
By Fourier transforming Eq.~(\ref{GenRes:xcorr1}) and introducing the power spectrum of the two observables
\begin{equation}\label{GenRes:PS}
\langle A(\vec{k}_a,\eta_a) B^*(\vec{k}_b,\eta_b) \rangle\equiv(2\pi)^3\delta(\vec{k}_a-\vec{k}_b)P_{AB}(k_a, \eta_a, \eta_b),
\end{equation}
it is straightforward to show that
\begin{eqnarray}
\langle\tilde{A}(\vec{x}_a)\tilde{B}(\vec{x}_b)\rangle&=&
\int\frac{d^3k}{(2\pi)^3}
e^{i\vec{k}\cdot(\vec{x}_a-\vec{x}_b)}P_{AB}(k, \eta_a, \eta_b)\nonumber\\
&\times&
\langle e^{i\vec{k}\cdot(\vec{\zeta}_a-\vec{\zeta}_b)}\rangle,
\label{GenRes:expcorrfunc}
\end{eqnarray}
assuming that the observables $A$, $B$ are uncorrelated with the lensing
deflection field $\vec{\zeta}$. Here $\eta_A$ and $\eta_B$ denote the conformal
times at which light was emitted at the sources to reach us today.

Equation (\ref{GenRes:expcorrfunc}) allows us to express the effect that weak lensing has on the unlensed correlation function. In other words, it quantifies the effect that the matter distribution -- responsible for lensing -- has on the observed distribution of the physical observables.
Note that the weak lensing modification depends only on the difference $\vec{\zeta}_a-\vec{\zeta}_b$
of the deflections in both observables, not on the absolute magnitude of each.
Assuming a flat Universe, as we do throughout, these distortions are given
by the following integrals along the line of sight:
\begin{eqnarray}
 \zeta_{a,\perp}^j&=&2\int_0^{\chi_a} d\chi(\chi_a-\chi)\nabla^j\Phi\left[\chi\vec\theta_a,\chi\right]\label{eq:perp}\\
\zeta_{a,\parallel}&=&-2\int_0^{\chi_a}d\chi\,\Phi\left[\chi\vec\theta_a,\chi\right] \label{eq:par}.
\end{eqnarray}
Here the subscripts $\perp$ and $\parallel$ indicate directions transverse
and parallel to the line of sight, respectively.
In the transverse case, there are two such direction, indexed here with $j=1,2$. The subscript $a$ refers to the position of the observable $A$, fully specified by the direction $\vec{\theta}_a$ and the comoving distance $\chi_a$. In the integral over $\chi$, the potential is to be evaluated along the line of sight so its argument is $\vec x(\chi)=[\chi\vec\theta_a,\chi]$ valid in the small angle limit we consider here. There is one important difference between the parallel distortion $\zeta_\parallel$ and the transverse distortion $\zeta_\perp$: the latter has an extra factor of $(\chi_a-\chi)\nabla$. The potential typically varies on small scales, so this factor is of order $\chi/r \gg 1$. The transverse distortion therefore produces the dominant change in correlation functions.

By neglecting all non-Gaussianity present in the lensing field, it is possible
to evaluate Eq.~(\ref{GenRes:expcorrfunc}) to
all orders, thus generalizing the results obtained by Challinor and Lewis
\cite{Lewis:2006fu} in the case of CMB lensing.
However, it is not clear to what extent this improves the
accuracy, since non-Gaussian terms, induced by gravity during structure
formation, appear in the expansion at all orders above
the second and may play a significant role especially at low redshift and
small scales. This issue can be resolved by tracing light rays through
N-body simulations of cosmological volumes (e.g., \cite{CarboneEtal}).
In the case of CMB lensing, there are indications that deviations from the
predictions of the calculation of \cite{Lewis:2006fu} which neglect
non-Gaussianities in the deflection field begin to appear at
$\ell \gtrsim 2000$ in the deflection field.
A detailed analysis of such a general treatment and of its
range of validity, requiring ray-tracing measurement of the probability
density function (PDF) of the displacements $\vec{\zeta}$, will be the focus
of a forthcoming work. We therefore briefly outline this general formalism
in appendix \ref{App:Exact} and for the rest of this work we will follow the
perturbative approach.

In order to proceed, we expand the exponential in Eq.~(\ref{GenRes:expcorrfunc})
to second order in the deflection. Note that all odd terms in this expansion
vanish due to symmetry, so that the expansion is good to fourth order. This is
sufficient to quantify the weak lensing impact on the correlation function
for sufficiently large separations.
Expanding Eq.~(\ref{GenRes:expcorrfunc}) above we then have
\begin{eqnarray}
\langle\tilde{A}\tilde{B}\rangle
&\approx &\langle A B\rangle
+ \frac{Z^{ij}}{r^2}
\nonumber\\
&\times&\left[ r_i r_j \frac{d^2 \langle AB\rangle}{dr^2}+ r\frac{d \langle AB\rangle}{dr}\left(\delta_{ij}-\frac{r_i r_j}{r^2}\right)\right],\label{GenRes:Corrfunctexpansion}
\end{eqnarray}
where $\vec{r}=\vec{x}_a-\vec{x}_b$ denotes the observed separation between the sources and the $3\times3$ distortion correlation tensor is defined as
\begin{eqnarray}
Z^{ij} &\equiv& \frac{\langle \zeta_a^i\zeta_a^j \rangle + \langle \zeta_b^i\zeta_b^j \rangle}{2}-\langle\zeta_a^i\zeta_b^j\rangle\nonumber\\
&\equiv&
\left(\begin{matrix}
 T-D/2 & 0 & -V_a\cr
0 & T+D/2 & 0 \cr
-V_b & 0 & S
\end{matrix}\right).
\label{Zdef}
\end{eqnarray}
The second definition here of the matrix elements holds if we choose $\vec x_a$ to lie along the $\hat z$ axis and both positions to lie in the $x-z$ plane, so that $\vec{x}_a$ and $\vec{x}_b$ have coordinates $\vec{x}_a=(0,0,\chi_a)$ and
$\vec{x}_b=(r_{\perp},0,\chi_a+r_{\parallel})$ respectively. Note that
due to the azimuthal symmetry of the lensing
displacements around the line of sight, we can always choose such coordinates without loss of generality.
In appendix \ref{App1} we derive expressions for the elements of the distortion tensor using the Limber approximation. The correlation of the distortions transverse to the line of sight decompose into a piece which is similar along both $x$ and $y$ directions
\begin{equation}
T(\chi,r_\parallel,r_\perp) = T_1(\chi,r_\parallel) + T_2(\chi,r_\perp)
\end{equation}
with
\begin{eqnarray}
T_1(\chi,r_\parallel) &\equiv& r_\parallel^2 \int_0^{\chi} d\chi' \int_0^\infty \frac{dk k^3P_\Phi(k,\chi')}{2\pi} \label{eq:t1}
\\
T_2(\chi,r_\perp)&\equiv &\int_0^{\chi} d\chi' \int_0^\infty \frac{dk k^3P_\Phi(k,\chi')}{\pi} (\chi-\chi')^2
\nonumber\\ &&\times
\left(1-J_0(kr_\perp\chi'/\chi)\right)\label{eq:t2}
\end{eqnarray}
and one which differs in the two transverse directions:
\begin{eqnarray}
D(\chi,r_\perp) &=& 2\int_0^{\chi} d\chi' (\chi-\chi')^2 \nonumber\\ &&\times\int_0^\infty \frac{dk k^3P_\Phi(k,\chi')}{\pi}
J_2(kr_\perp\chi'/\chi).\label{eq:d}
\end{eqnarray}
Note that both $T_2$ and $D$, which depend only on the transverse distance between the two background objects, vanish in the limit that $r_\perp=0$. Since we will see that these two terms dominate the distortion of the correlation function, changes to the correlation functions have a characteristic dependence on the
\textit{projected} separation $r_\perp$, peaking when $r_\perp=r$.
The variance of the displacements along the line of sight due to time delay is:
\begin{eqnarray}
S(\chi,r_\perp) &=& 2\int_0^\chi d\chi' \int_0^\infty \frac{dk\,k P(k,\chi')}{\pi}\nonumber\\ &&\times\left[1-J_0(kr_\perp \chi'/\chi)\right].\label{eq:s}
\end{eqnarray}
Finally, the displacement along the line of sight is slightly correlated with the transverse distortion; the relevant combination is
\begin{equation}
V_a+V_b=2r_\parallel \int_0^\chi d\chi' \int_0^\infty \frac{dk\,k^2 P(k,\chi')}{\pi} J_1(kr_\perp \chi'/\chi).
\end{equation}

It is useful to estimate the order of magnitude of the corrections. First
consider Eqs.~(\ref{eq:perp}, \ref{eq:par}). The RMS of the perpendicular
distortion is of order $\Phi_{\rm RMS} \chi^2/r$, where $\chi$ is a
typical cosmological distance, of order a Gpc, and $r$ is a typical distance
over which the potential varies, typically much smaller. The RMS of the
parallel distortion is seen to be smaller by a factor of $(r/\chi)$. These
estimates translate well into the respective variances as encoded in the
functions $T_2$ and $D$. Both $T_2$ and $D$ are seen from Eqs.~(\ref{eq:t2},
\ref{eq:d}) to be of order $k^3P_\Phi(k) k\chi^3$ since the line of sight
variable $\chi'$ is order $\chi$.  The variance of the gravitational potential
is roughly $\Delta^2_\Phi(k)\sim k^3P_\Phi(k)$, and the $k$ integral picks
out values of $k\sim r^{-1}$. So both $T_2$ and $D$ are of order
$\Delta^2_\Phi(1/r) (\chi^2/r)^2\times (r/\chi)$, where $\Delta^2_\Phi(k)$
is equal to $\Phi_{\rm RMS}^2 \sim 10^{-9}$ on large scales
($k\lesssim 0.01h/\mbox{Mpc}$) and suppressed on smaller scales due to the transfer
function. The extra factor of $r/\chi$
is the standard Limber suppression due to cancellation along the line of
sight (only modes with $k_z$ small contribute to the variance).
On large scales, the relevant dimensionless quantities $T_2/r^2$, $D/r^2$
thus are of order $\Phi_{\rm RMS}^2 \chi^3/r^3 \sim 10^{-6}\, (100\:\mbox{Mpc}/h/r)^3$.
They increase towards small scales, however not as quickly as $r^{-3}$, since
the variance of the potential is suppressed by the transfer
function towards smaller scales. In other words, due to the suppressed power
on small scales,
photons from both directions are deflected more and more coherently, and
$r_{obs}$ is very close to $r$ which is reflected by reduced values
of $T_2$ and $D$.

The first term in the transverse deflection correlation,
$T_1$ as defined in Eq.~(\ref{eq:t1}), represents the difference between the
lensing experienced by A and B due to their different distances from us, so
this part of the transverse lensing is suppressed by a factor of
$r_\parallel^2/\chi^2$ and can usually be neglected. Similar estimates show
that $S$ and $V_a+V_b$ are both smaller than the transverse variances $T_2$
and $D$ by a factor of $(r/\chi)^2$ as expected from a cursory examination
of Eqs.~(\ref{eq:perp},\ref{eq:par}). So we expect, and numerical work
confirms this, that $T_2$ and $D$ dominate the corrections to correlation
functions, and the corrections will be of order
$\Delta^2_\Phi(1/r) (\chi/r)^3$.

Therefore, corrections to cosmological correlations due to weak lensing are small and given by:
\begin{eqnarray}
\langle\tilde{A}\tilde{B}\rangle(r,r_\perp,\chi)
\approx
\langle A B\rangle(r,\chi)
+ T_2(\chi,r_\perp)\frac{2}{r}\frac{d\langle AB\rangle}{dr}
 \nonumber\\
+\left(T_2(\chi,r_\perp)-\frac{D(\chi,r_\perp)}{2}\right) \frac{r_\perp^2}{r^2} r \frac{d}{dr}\left[
\frac{1}{r}\frac{d\langle AB\rangle}{dr}\right].\nonumber\\
\label{GenRes:LH}
\end{eqnarray}
Two general features of this equation are worth pointing out: first, if the
correlation function is close to a pure power-law, both derivative terms
will be of order $\langle AB\rangle/r^2$. Hence, the relative
lensing-induced effect on the correlation function will be given by
$T_2/r^2$ and $D/r^2$, which are shown in Fig.~\ref{fig:Ta} and \ref{fig:d}.
Second, in case of an oscillating correlation function, the lensing
contribution can be amplified by large values of $d\langle AB\rangle/dr$
and $d^2\langle AB\rangle/dr^2$. Further,
lensing will tend to smooth out the oscillations: at a local minimum of $\langle AB\rangle$,
the first derivative vanishes, while the second derivative is positive,
so that the observed correlation is increased by lensing. At a local maximum,
the opposite holds.
This feature is already well-known in $\ell$-space in case of the CMB.

Equation (\ref{GenRes:LH}) holds for any cosmological correlation function. It applies equally well to point-like sources and to diffuse backgrounds, to galaxies and QSO, to CMB and to the 21-cm radiation (albeit in the case of discrete sources magnification bias effects might provide the dominant distortion of the correlation function). Given a particular matter distribution, it is sufficient to evaluate the functions $T_2$ and $D$ \textit{once} to be able to calculate the effect that weak lensing has on the correlation function of \textit{any} cosmological observable.

\begin{figure}
\includegraphics[width=0.49\textwidth]{T2_0311.eps}
\caption{Contour plot of $T_2/r^2$ [Eq.~(\ref{eq:t2})] determining the relative transverse
displacement as a function of the source separation $r$ and source redshift $z$
(assumed
equal for both sources, so $r_\perp=r$).  }\label{fig:Ta}
\end{figure}

\begin{figure}
\includegraphics[width=0.49\textwidth]{D_0311.eps}
\caption{Same as Fig.~\ref{fig:Ta} but for $D/r^2$, where $D$ is defined in Eq.~(\ref{eq:d}). }\label{fig:d}
\end{figure}

The functions $T_2/r^2$ and $D/r^2$ are shown for a concordance $\Lambda$CDM cosmology with $\Omega_m=0.3$ and $\Omega_{\Lambda}=0.7$ (which will be assumed throughout) in Figs.~\ref{fig:Ta} and \ref{fig:d}. We used the non-linear
matter power spectrum from \texttt{halofit} \cite{halofit} in the calculation.
As the positions $A$ and $B$ move out to higher redshift, the lensing effects become larger since the longer path lengths lead to larger RMS deflections. At
fixed redshift, both $T_2$ and $D$ become larger as $r$ gets bigger since the
displacements of the path from the two points to us cease to be correlated and
hence experience independent deflections. However, as discussed above, the
relative effect of lensing distortions will generically be of order $T_2/r^2$,
$D/r^2$. These quantities decrease as
$r$ increases, as illustrated in Figs.~\ref{fig:Ta} and \ref{fig:d}. Hence,
in the absence of features in the unlensed correlation function considered,
the effect of lensing is likely to be most important on small scales. Since
the perturbative expansion treatment we are using is valid under the condition
that $(T_2/r^2,D/r^2) \ll 1$,  Figs.~\ref{fig:Ta} and \ref{fig:d} illustrate
that the approximation used here is always applicable: it will yield a good
approximation to the size of the lensing effect. If the effect is only
marginally observable, this approximation should be sufficient. If however
the desired precision on lensing effect itself is high, as, e.g. in the case
of CMB lensing in order to improve cosmological parameter constraints,
higher-order corrections will have to be taken into account.

The value of the correlator of the longitudinal displacements $S/r^2 = Z^{33}/r^2$
is shown in Fig.~\ref{fig:Sab}. The longitudinal displacement effect (time delay) is clearly much smaller than the perpendicular one, as found earlier in \cite{CoorayHu}.
\begin{figure}
\includegraphics[width=0.49\textwidth]{S_0526.eps}
\caption{Contour plot of $S/r^2$ [Eq.~(\ref{eq:s})] determining the relative longitudinal
displacement as a function of the source separation $r$ and source redshift $z$
(assumed
equal for both sources). }\label{fig:Sab}
\end{figure}

\section{Applications}\label{Sec:Apps}

We are now in a position to apply the above results to the correlation function of three different kinds of sources: galaxies, the CMB, and the 21-cm radiation background. The CMB is an angular measurement so all photons come from the same comoving distance meaning that $r_\parallel=0$ and the dependence is solely on $r=r_\perp$. For galaxies and 21cm, the orientation of the radius vector with respect to the line of sight is a free parameter, so the smoothing depends on
$r_\perp$ even when $r$ is fixed.

\subsection{Galaxies}

The effect of weak lensing on the galaxy correlation function has been taken into account in previous work in the context of the analysis of the impact that lensing has on the determination of the sound horizon of baryon oscillations \cite{Vallinotto:2007mf}. The ratio of the lensing induced term to the unlensed correlation function is plotted in Fig.~\ref{fig:NewBao}. Lensing smoothes the BAO bump at the percent level.
Note that since the lensing effect multiplies derivatives of the unlensed
correlation function, the relative effect of lensing will be independent of
any galaxy bias, in contrast to the magnification bias, whose relative effect
is $\propto 1/b$ or $\propto 1/b^2$, depending on redshift \cite{Hui:2007cu}.
We point out that Eqs.~(6-8) of \cite{Vallinotto:2007mf} are recovered using Eq.~(\ref{GenRes:LH}) above once the dependence of the kernels on the angle $\theta$ is correctly taken into account in \cite{Vallinotto:2007mf}.

\begin{figure}[ht]
\includegraphics[width=0.49\textwidth]{big_xi_Bao_ok.eps}
\caption{Relative deviation from the unlensed correlation function of the
galaxy correlation function including effects of lensing deflections,
near the baryon acoustic scale. Lensing smoothes the BAO feature in the
galaxy correlation function at the percent level.} \label{fig:NewBao}
\end{figure}

Fig.~\ref{fig:deltaxi} shows the angular dependence of the correlation function for galaxies at redshift 3. The characteristic angular dependence illustrated in Fig.~\ref{fig:deltaxi} may make this effect detectable. Note that due to
the smallness of the time-delay effect ($S/r^2$, Fig.~\ref{fig:Sab}), the
lensing contribution essentially vanishes for $\alpha\rightarrow0$.

\begin{figure}[ht]
\includegraphics[width=0.49\textwidth]{deltaxi-DSV.eps}
\caption{Difference between the lensed and unlensed matter correlation
function
at $z=3$ near the BAO feature. The three lines shown are for different
orientations of the radius vector with respect to the line of sight: perpendicular (solid/red), at 45$^{\circ}$ (dotted/green), and parallel to the line of sight
(dashed/blue). The lensing contribution shows a strong dependence on the
orientation of the separation vector.} \label{fig:deltaxi}
\end{figure}

\subsection{Cosmic Microwave Background}

The smoothing effect of lensing on the CMB power spectrum was computed long ago~\cite{Seljak:1995ve} in multipole space. The formalism established here allows for a simple calculation of this same effect in angular space.

The angular temperature correlation function of the CMB
is given by:
\begin{equation}
w_{TT}(\theta) = \sum_{l=2}^{\infty} \frac{2l+1}{4\pi}
C^{TT}(l)\:P_l(\cos\theta),
\label{eq:wTT}
\end{equation}
where $P_l$ denote the Legendre polynomials.
Applying the approach presented here, we can calculate the
lensing effect on the angular correlation function by
evaluating Eq.~(\ref{GenRes:LH}). Then, $\langle AB \rangle(r)$ stands for the
temperature correlation function $\xi_{TT}(r) = w_{TT}(r/\chi_{*})$, where
$\chi_{*}$ is the distance to the last scattering surface.
For this, we need the first and second derivatives of  $\xi_{TT}(r)$ which
are given by:
\begin{eqnarray}
\frac{d}{dr} \xi_{TT}(r) &=& \frac{-\sin\theta}{\chi_{*}} \frac{d
w_{TT}}{d\cos\theta} \nonumber \\
\frac{d^2}{dr^2} \xi_{TT}(r) &=& \frac{-\cos\theta}{\chi_{*}^2} \frac{d
w_{TT}}{d\cos\theta} + \frac{\sin^2\theta}{\chi_{*}^2} \frac{d^2
w_{TT}}{d\cos\theta^2}
\label{eq:xiTT}
\end{eqnarray}
The derivatives of $w_{TT}$ with respect to $\cos\theta$ can be carried out using
the Legendre polynomial relation:
\begin{equation}
P_l'(x) = \frac{l}{x^2-1} ( x P_{l}(x) - P_{l-1}(x) )
\end{equation}

Fig.~\ref{fig:CMBlensing1} shows the lensed and unlensed CMB angular
correlation functions in the region of the baryon acoustic feature.
One can discern a slight smoothing effect of lensing in real space, as
pointed out after Eq.~(\ref{GenRes:LH}).
Fig.~\ref{fig:CMBlensing2} shows the difference between the lensed and
unlensed correlation functions calculated in this approach (thick line). The
unlensed $C^{TT}(l)$ were obtained from CAMB \cite{Lewis:1999bs}.
In the figure we also show the correlation function obtained from the
lensed $C^{TT}(l)$ given by CAMB using Eq.~(\ref{eq:wTT}) (thin line).
Clearly, the calculations in the two different approaches agree for $\theta \gtrsim 0.1^{\circ}$
corresponding to $r \gtrsim 15\mbox{Mpc}/h$. Note that results from N-body simulations
\cite{CarboneEtal} show deviations from the results of the CAMB code
for $\ell \gtrsim 2000$, roughly corresponding to $\theta \lesssim 0.03^{\circ}$;
however, it is not straightforward to convert the scale where deviations
appear in multipole space to a corresponding angular scale in real space.

\begin{figure}[ht]
\includegraphics[width=0.49\textwidth]{wCMB.eps}
\caption{Lensed (solid) and unlensed (dotted) CMB angular correlation functions.A slight smoothing effect washing out the baryon acoustic feature can be
seen. \label{fig:CMBlensing1}}
\end{figure}

\begin{figure}[ht]
\includegraphics[width=0.49\textwidth]{delta-wCMB-NL.eps}
\caption{Difference between the lensed and unlensed CMB angular correlation
function $w_{TT}(\theta)$. The thick line shows the calculation
using the first-order approach presented here, while the thin line is
the lensed $w_{TT}$ obtained from CAMB.\label{fig:CMBlensing2}}
\end{figure}

\subsection{21-cm Surveys}

In principle, redshifted 21 cm radiation encodes information about the 3D distribution of neutral hydrogen in the universe. This distribution is sensitive to both inhomogeneities in the matter and in the free electron density. It is not our purpose here to compute the complicated correlation function that results. Rather, we note that the real space calculation presented here is particularly simple to apply to any model of reionization (see Ref.~\cite{Mandel:2005xh} for a careful discussion of the complications that arise in Fourier space).

For the purposes of this paper, we use the 21cm predictions for the ``dark ages''
before reionization calculated in \cite{Lewis21cm}. We use the 21cm spin temperature
correlation coefficients $C^{TT}(\ell)$ at $z=50$, in the same way as
outlined above in the case of the CMB.
Fig.~\ref{fig:21cm} shows the relative lensing effect on the 21cm angular
correlation function. It is rather small compared to that of the CMB
due to the overall smoothness of the 21cm angular correlation function
in the dark ages. Note that at lower redshifts, $z\lesssim 12$, we expect
the 21cm correlation function to show a stronger baryonic signature
\cite{Wyithe:2007rq}, and hence expect a higher lensing effect possibly of
importance to cosmological parameter constraints
\cite{McQuinn:2005hk,Bowman:2005hj,Santos:2006fp,Mao:2008ug}.

\begin{figure}[t]
\includegraphics[width=0.49\textwidth]{reldelta-w21cm.eps}
\caption{Relative lensing effect on the angular correlation function
of 21cm emission from the dark ages. We use the cross-correlation coefficients
from \cite{Lewis21cm}. The redshift is $z=50$, and the bandwidth chosen
is 0.01~MHz.}
 \label{fig:21cm}
\end{figure}

\section{Discussion}\label{Sec:Conclusions}

Gravitational lensing affects cosmological correlation functions in two ways. First, since the geodesics which photons travel on are sensitive to the distribution of matter between source and observer and since the latter is locally inhomogeneous thanks to structure formation, weak lensing acts by displacing the sources' observed (as opposed to true) positions. The correlation function that is measured from observed data therefore also includes the contribution from these lensing deflections. Second, weak lensing also acts on observations by focusing or defocusing the geodesics' congruences, thus altering the observed brightness of a source. This latter effect, known as \textit{magnification bias}, is generally larger than the former \cite{Matsubara2000,Hui:2007cu} but it applies only to pointlike sources (see e.g. \cite{Hui:2007cu, Vallinotto:2007mf, Schmidt:2008mb} for studies
of the effect of magnification bias on two- and three-point correlation
functions). Both these effects are small but potentially relevant in the present age of precision cosmology. In this work we focused on the first of these effects and we derived a \textit{general} perturbative formula that can be used to quantify it.

The results of the present work depend only on the following two assumptions: that photons travel on geodesics and that higher order corrections to the correlation function (arising from higher order correlators of the lensing induced displacements) can safely be neglected. The first of this assumption has two consequences of opposite nature. The positive consequence is that the result obtained in this work is general and applies to \textit{any} cosmological correlation function, regardless of the nature of the source and of the physical observables that are being measured and correlated. Moreover, the correction terms that appear in Eq.~(\ref{GenRes:LH}) and that quantify the effect of lensing depend only on the power spectrum of matter: given a specific cosmological model they need to be evaluated only once and they can then be applied to any correlation function. As such, they also represent a map that will tell whether weak lensing will have a relevant or an irrelevant role in the measurement of a given correlation function \textit{before} the actual measurement is carried out. The negative consequence, on the other hand, is that this lensing-induced distortions represent a theoretical systematic that will \textit{always} be present regardless of the precision of the instruments used to carry out the observation. In other words, even if ``perfect observations'' free of any systematics could be carried out, this lensing-induced noise would still creep into the correlation function that would be calculated using those data. This lensing-induced modification of the correlation may be avoided only by reconstructing a map of the lensing
potential (e.g., \cite{Hirata:2002jy}). Another avenue to a possible disentanglement of this lensing distortion from the observed correlation function -- at least for sources that are not confined to a fixed redshift -- could be to exploit the angular dependence of the effect as seen in Fig.~\ref{fig:deltaxi}. Furthermore, since the lensing modification depends on the derivatives of the correlation function, correlation functions that are rapidly oscillating will in general be most affected by lensing, i.e. the features will be somewhat smoothed. Conversely, in quantities that are intrinsically uncorrelated, no correlation will be induced by lensing deflections.

The second assumption entering the derivation of Eq.~(\ref{GenRes:LH}) is that terms of third and higher order are discarded when the exponential of Eq.~(\ref{GenRes:expcorrfunc}) is expanded. As shown in Appendix \ref{App1}, this assumption corresponds to Taylor expanding the coordinate dependence of the physical observables and to retain only terms up to second order, which in turn corresponds to neglecting all contributions arising from the non-Gaussianity of the displacements' PDF. Despite the fact that under the same assumptions the general formalism outlined in Appendix \ref{App:Exact} can be used to calculate the lensing distortion arising from the sum of \textit{all} the terms appearing in the exponential of Eq.~(\ref{GenRes:expcorrfunc}), it is however unclear to what extent this might really represent an improvement. If on one hand the sum of all the terms appearing in the exponential may give important contributions on small scales, it is also true that on such small scales departures from gaussianity of the displacements' PDF -- induced by the non-linear growth of structure at low redshift -- could play a relevant role. The range of applicability of such a non-perturbative method and the gain in precision that it would allow on small scales are the focus of a current project.

\acknowledgments
AV is supported by Agence Nationale de la Recherche (ANR). AV thanks Carlo Schimd, Emiliano Sefusatti and Jean-Philippe Uzan for useful discussions and comments. SD
is supported by the Fermi Research Alliance, LLC under Contract No. DE-AC02-07CH11359 with the US Department of Energy.
FS thanks Wayne Hu for helpful discussions, and is
supported by the Kavli Institute for Cosmological Physics at the University of Chicago through grants NSF PHY-0114422 and NSF PHY-0551142 and an endowment from the Kavli Foundation and its founder Fred Kavli.

redpajama_set_name: RedPajamaArXiv


Nicola Schutte is an Associate Professor of Psychology at the University of New England in New South Wales, Australia. Her research interests lie in the areas of positive psychology, with an emphasis on emotional intelligence, self-efficacy, and the effects of positive affect. She has co-authored several books and over 80 chapters and research articles. Her books include: Schutte, N.S. & Malouff, J.M. (1995) Sourcebook of adult assessment strategies (Plenum); Malouff, J.M. & Schutte, N.S. (1998) Games to enhance social and emotional skills: Sixty‑six games that teach children, adolescents, and adults skills crucial to success in life (Charles C Thomas); Schutte, N.S. & Malouff, J.M. (1999) Measuring emotional intelligence and related constructs (Edwin Mellen); Schutte, N.S. & Malouff, J.M. (2006). Why we read and how reading transforms us (Edwin Mellen); and Malouff, J.M. & Schutte, N.S. (2007). Activities to teach social, emotional and problem solving skills, 2nd edition (Charles C Thomas Press). Her research in the area of emotional intelligence focuses on the measurement of emotional intelligence, the relationship between emotional intelligence and important intra and inter-personal characteristics and approaches to increasing emotional intelligence.
Schutte, N. S. , Malouff, J. M., Hall, L. E., Haggerty, D., Cooper, J. T., Golden, C., & Dornheim, L. (1998). Development and validation of a measure of emotional intelligence. Personality and Individual Differences, 25, 167-177.
Schutte, N.S., Malouff, J.M., Bobik, C., Conston, T., Greeson, C., Jedlicka, C., Rhodes, E. & Wendorf, G. (2001). Emotional intelligence and interpersonal relations. Journal of Social Psychology, 141, 523-536.
Schutte, N. S., Schuettpelz, E, & Malouff, J. M. (2001). Emotional intelligence and task performance. Imagination, Cognition, and Personality, 20, 347-354.
Schutte, N.S. & Malouff, J.M. (2002). Incorporating emotional skills in a college transition course enhances student retention. Journal of the First-Year Experience and Students in Transition, 14, 7-21.
Schutte, N.S., Malouff, J.M., Simunek, M., Hollander, S., & McKenley, J. (2002). Characteristic emotional intelligence and emotional well-being. Cognition and Emotion, 16, 769-785.
Riley, H. & Schutte, N.S. (2003). Low emotional intelligence as a predictor of substance-use problems. Journal of Drug Education, 33, 391-398.
Kernbach, S. & Schutte, N.S. (2005). The impact of service providers' emotional intelligence on customer satisfaction. Journal of Services Marketing, 19, 438-441.
Schutte, N.S. (2006). Techniques for developing emotional intelligence. In Stough, C., Saklofske, D. & Hansen, K (Eds.). Research on Emotional Intelligence: International Symposium 2005 (pp 77-88), Melbourne Australia, Tertiary Press.
Wing, J.F., Schutte, N.S., & Byrne, B. (2006). The effect of positive writing on emotional intelligence and life satisfaction. Journal of Clinical Psychology, 62(10), 1291-1302.
Brown, R. F. & Schutte, N.S. (2006). Direct and indirect relationships between emotional intelligence and subjective fatigue in university students. Journal of Psychosomatic Research, 60, 585-93.
Sillick, T. J. & Schutte, N.S. (2006). Emotional intelligence and self-esteem mediate between perceived early parental love and adult happiness. E-Journal of Applied Psychology,2, 38-48.
Kaur, I., Schutte, N.S., & Thorsteinsson, E.B. (2006). Gambling control self-efficacy as a mediator of the effects of low emotional intelligence on problem gambling. Journal of Gambling Studies, 22, 405-411.
Schutte, N.S., Malouff, J.M., Thorsteinsson, E.B., Bhullar, N. & Rooke, S.E., (2007). A meta-analytic investigation of the relationship between emotional intelligence and health. Personality and Individual Differences, 42, 921-933.
Schutte, N.S, Malouff, J.M., Price, I., Walter, S., Burke, G., & Wilkinson, C. (2008). Person-situation interaction in adaptive emotional functioning. Current Psychology, 27, 112-111.
Kirk, B.A., Schutte, N.S., & Hine, D.W. (2008). Development and preliminary validation of an emotional self-efficacy scale. Personality and Individual Differences, 45, 432–436.
Schutte, N., Malouff, J., & Brown, R. (2008). Efficacy of an emotion-focused treatment for prolonged fatigue. Behavior Modification, 32, 699-713.
Schutte, N.S., Manes, R.R., & Malouff, J.M. (2009). Antecedent-focused emotion regulation, response modulation and well-being. Current Psychology, 28, 21-31.
Kirk, B.A., Schutte, N.S., & Hine, D.W. (2009). The role of emotional self efficacy, emotional intelligence and affect in workplace incivility and workplace satisfaction. In C. E. J. Hartel, N. M. Ashkanasy & W. J. Zerbe (Eds), Research on Emotions in Organizations – Volume 5: Emotions in Groups, Organizations and Cultures. 213-230.
Schutte, N.S., Thorsteinsson, E.B., Hine, D.W. Foster, R., Cauchi, A., & Binns, C. (2010). Experiential and Rational Processing Styles, Emotional Intelligence and Well-Being. Australian Journal of Psychology, 62, 14 - 19.
Schutte, N. (2010). Conexiones entre Inteligencia Emocional y los Procesos e Regulación Emocional. En R. Sánchez Aragón (Ed.) Regulación Emocional: Una Travesía de la Cultura al Desarrollo de las Relaciones Personales (pp. 35-45). México: Universidad Nacional Autónoma de México.


Lana Popham did her homework in preparation for a presentation to the Capital Regional District board. Popham is lobbying for an all-out ban on disposable plastic bags from the region.
She collected statistics and signatures, did interviews and gave herself a pep talk.
It all culminated in eight minutes in front of the Solid Waste Advisory Committee in December. The Saanich resident was allowed to state her case only to learn she was presenting to the wrong audience.
"They told me that it was not a CRD issue and it was up to individual municipalities," Popham said.
Despite the minor setback, her crusade isn't over. Popham has scheduled a meeting with the municipality of North Saanich in January to make her presentation there.
She'll move on to the region's 12 other municipalities, asking each to ban plastic bags.
In fact, Popham should have started her quest in front of individual municipalities, says Saanich's municipal solicitor Chris Nation.
"Municipal council would do a consultation with the business community - grocery and retail stores that use plastic bags," Nation said.
Forming a bylaw, Nation said, wouldn't have to go through a formal public hearing process.
Rather, councillors would either push it though or shut it down at a council meeting.
Popham has also asked to meet with the municipality of Saanich "as soon as possible" to get talking about the ban.


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Courthope History, Family Crest & Coats of Arms
The ancient roots of the Courthope family name are in the Anglo-Saxon culture. The name Courthope comes from when the family lived in the village of Courthope in the county of Sussex.
Early Origins of the Courthope family
The surname Courthope was first found in Sussex, where "from the reign of King Edward I., this family has been settled at Wadhurst, Lamberhurst, Ticehurst, and the adjoining parishes on the borders of Sussex and Kent." [1]
Continuing, the "first [record of the name] occurs in a Subsidy Roll at Wadhurst, co. Sussex, in exactly it's present form [Courthope], temp. Edward I." [2]
Early History of the Courthope family
This web page shows only a small excerpt of our Courthope research. Another 103 words (7 lines of text) covering the years 1296, 1592, 1628, 1632, 1681, 1616, 1685, 1656, 1620, 1609 and 1616 are included under the topic Early Courthope History in all our PDF Extended History products and printed products wherever possible.
Courthope Spelling Variations
One relatively recent invention that did much to standardize English spelling was the printing press. However, before its invention even the most literate people recorded their names according to sound rather than spelling. The spelling variations under which the name Courthope has appeared include Courthope, Curtehope, Courtopp, Courthop and many more.
Early Notables of the Courthope family (pre 1700)
Distinguished members of the family include William de Curtehope, a prominent landholder in 13th century Sussex; and Sir George Courthorpe (1616-1685), an English politician, Member of Parliament for Sussex (1656.) Nathaniel Courthopp (d. 1620), was an English sea-captain in the service of the East India Company who enlisted in the company's service in November 1609, and left England in the Darling, one of Sir H. Middleton's fleet. With his commander and others he...
Another 72 words (5 lines of text) are included under the topic Early Courthope Notables in all our PDF Extended History products and printed products wherever possible.
Migration of the Courthope family
At this time, the shores of the New World beckoned many English families that felt that the social climate in England was oppressive and lacked opportunity for change. Thousands left England at great expense in ships that were overcrowded and full of disease. A great portion of these settlers never survived the journey and even a greater number arrived sick, starving, and without a penny. The survivors, however, were often greeted with greater opportunity than they could have experienced back home. These English settlers made significant contributions to those colonies that would eventually become the United States and Canada. An examination of early immigration records and passenger ship lists revealed that people bearing the name Courthope arrived in North America very early: a number of settlers who arrived in the New World by the 19th century.
Contemporary Notables of the name Courthope (post 1700) +
William Courthope (1842-1917), English writer and historian of poetry
William John Courthope (1842-1917), English poet/critic
George Lloyd Courthope, 1st Baron Courthope
Courthope (English)