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aspca commercial narrator 2020
These famous faces are celebrating in December. Starting in 2010, Hamm scored a plum gig when he became the voice of Mercedes-Benz, lending some gravitas and style to the luxury car's commercials. What are the disadvantages of primary group? The Hunger Games and The Devil Wears Prada star is the familiar-sounding voice behind AT&T's "Raising the Bar" campaign, rolled out following the AT&T–Cingular Wireless merger in 2004. If you felt like the voice in the Walgreens commercials reminding you how much cash you could save with Medicare Part D sounded familiar, you're right. Live smarter, look better, and live your life to the absolute fullest. Narrator of the ASPCA commercials. Jon Hamm may be best known for his role as Don Draper on AMC hit Mad Men from 2007 to 2015, but that's far from the only trick the actor has had up his sleeve. If you've ever watched a television commercial and felt for sure that you knew the voice-over artist from somewhere, chances are, you're right. ASPCA To Celebrate 22nd Annual Bergh Ball Apr 25, 2019 Ashley Greene Supporting the ASPCA in Disaster Relief Efforts Dec 7, 2018 The ASPCA To Host 2018 Humane Awards Luncheon Nov 13, 2018 Reach him at max.garland@commercialappeal.com or 901-529-2651 and on Twitter @MaxGarlandTypes . )- Something so sad, that will make almost anyone anyone cry till they die. While Simmons' booming voice is generally highly recognizable, the actor tapped into his skill as a thespian, completely disguising himself as the naïve goofball M&M in both commercials and I Lost My M in Vegas, a 3D movie that can be seen at the M&Ms World store in Las Vegas. What they do Make arrests for crimes against animals Caring for pet parents and pets Providing positive outcomes for at-risk animals serving victims of animal cruelty Appeal 1 This commercial appeals to people, mostly animal lovers, because it's showing sad faces of dogs and She received nominations for the Academy Award for Best Supporting Actress for her roles in the comedy-drama Working Girl (1988) and the romantic comedy In & … However, this is far from the only voice-over work on Dafoe's résumé: he's also voiced roles in Fantastic Mr. Fox, Finding Nemo, Finding Dory, and The Simpsons. 2020-10-01 19:40:49 2020-10-01 19:40:49. The Arrested Development star has also lent his distinctive sound to a series of commercials for GMC trucks. We each worked more than full-time last year for $9.71 an hour in wages and benefits, serving more than 573,000 readers –– and ANIMALS 24-7 still ended up $7,800 in the hole, because, unfortunately, not enough of those readers elected to make us one of their choices to get their eight bucks a month, or whatever, mostly not through any dissatisfaction with us or the work we do. In line with their love of animals, Subaru counts the ASPCA among one of the beneficiaries of Share the Love, contributing to the rescue, adoption and transport of 50,000 animals. With seven years playing a blood splatter expert and serial killer on Dexter under his belt, Michael C. Hall must have seemed like a perfect choice for Dodge's surprisingly dark "Leader of the Human Resistance" commercials. Who is the longest reigning WWE Champion of all time? Mostly dark colors are shown in the commercial, which sometimes tend to make people feel depressed in some way. I think it's Bonnie Hunt, but I haven't validated my answer. While Breaking Bad fans are all-too-familiar with his iconic, albeit vulgar, catchphrase from the AMC hit, Aaron Paul proved he's capable of a more sophisticated tone with advertisements for Cadillac. Back in 1999, communications company Qwest tapped Willem Dafoe to lend his unique voice to their commercial in which a man finds himself stranded at a roadside motel offering little in the way of amenities—with the exception of every movie ever made on TV, thanks to Qwest. Charity Navigator calculates that ASPCA spent a whopping $52 million on fundraising in 2012. These hilarious celebrities are laughing through the pain of parenthood. And for more surprising celebrity roles, discover these 11 Times A-List Celebrities Became Real-Life Heroes. Morgan Freeman's smooth, deep voice is one of the most recognizable in Hollywood, and that's just what Visa was counting on when they tapped the Oscar-winning actor to do voice-overs for them. 1)aspca commercial(adj. All Rights Reserved. When did organ music become associated with baseball? How long will the footprints on the moon last? The first animal hospitals under ASPCA were created in 1912. To discover more amazing secrets about living your best life, click here to follow us on Instagram! Ethos is an appeal to character, meaning it is a process of convincing the audi-ence of the character and credibility of the persuader.In the commercial, they used a famous singer, Sarah McLachlan, to speak to the audience to have that much more of an impact on them. New ASPCA Commercial. © 2020 Galvanized Media. Even the colors in the advertisement have an effect on the viewer. Ross Huguet is a Voice Actor in North America... Ross Huguet carries a confident, arresting and hypnotic voice that's warm and convincingly trustworthy. Even Sarah McLachlan changes the channel when her notoriously gut-wrenching ASPCA commercials come on. However, Visa isn't the only company that's used Freeman's distinctive sound to advertise their products: the 80-year-old actor has also done a series of commercials for the NFL. If you've ever gotten "Smelly Cat" stuck in your head while a Yoplait commercial played, you're not alone. If you've ever wondered why those Tylenol ads telling you to ride your bike, go swimming with your grandkids, or run a 5K are so convincing, it might just be the star behind them. We work to rescue animals from abuse, pass humane laws and… If you've ever wondered why the voice yelling, "We have the meats!" 18 Oct 2020 Plaque installed by Thai protesters near palace removed The plaque featured the three-fingered salute of the protest movement and said Thailand belonged to its people. Zach Braff hasn't limited his roles outside of Scrubs to whimsical indie movies. Copyright © 2020 Multiply Media, LLC. at you in the Arby's ads sounded cool, it's because the commercials are voiced by none other than Pulp Fiction and Mission Impossible star Ving Rhames. Watch, interact and learn more about the songs, characters, and celebrities that appear in your favorite ASPCA TV Commercials. Joan Mary Cusack (/ ˈ k juː s æ k /; born October 11, 1962) is an American actress and comedian. In a year full of changes, Thanksgiving will also be altered for 2020. Bestlifeonline.com is part of the Meredith Health Group, All of the reasons why stars are definitely. Browse more videos. This is an approach to advertising's effects on the society. The PSAs have taken on a life of their own because of how hard they can be to watch. One of the rhetorical devices the ASPCA commercial uses to help persuade the targeted audience is ethos. The effectiveness of this commercial is proven, simply by watching the reactions of the commercial's viewers. Experts say lengthy showers aren't good for you. The famed singer has lent her voice to numerous commercials sponsored by the American Society For The Prevention Of Cruelty to Animals that feature sad-looking animals desperate for a home. The yogurt brand's "It Is So Good" commercials are voiced by none other than Friends star Lisa Kudrow, who has been doing voice acting for years, including a recent recurring role on Netflix's animated series Bojack Horseman. Along with these scenes is a touching song playing in the background. Enter your email address to get the best tips and advice. Who does the voice over for aspca tv commercial? A free inside look at company reviews and salaries posted anonymously by employees. When did Elizabeth Berkley get a gap between her front teeth? How tall are the members of lady antebellum? He has a super sexy voice! In 2014, Rudd signed on as the voice-over artist for Hyundai, lending his somewhat anonymous sound to the car company's commercials. ASPCA TV Commercial, 'The Next Minute' Ad ID: 2732932 60s 2020 ( Inactive ) SHOW MORE. After years of playing Special Agent Fox Mulder on The X-Files, David Duchovny took on a decidedly less-spooky (and less visible) role. Is it Sarah McLachlan? Emmy winner Stanley Tucci may be best known for his dramatic work on the big screen, but he's also got an impressive commercial portfolio under his belt, too. American Society for the Prevention of Cruelty to Animals is a Animal Rights, Welfare, and Services charity located in New York, NY. The material on this site can not be reproduced, distributed, transmitted, cached or otherwise used, except with prior written permission of Multiply. Since the creation of these hospitals, ASPCA found a new tactic in improving its cause: the ability to develop various medical procedures and innovations with help from new discoveries in medicine and technology. Their latest commercial highlights this special relationship, showing a little girl falling for a … And for more insight on your favorite celebs, brush up on the 30 Funniest Photos of Celebrities as Teens. How old was queen elizabeth 2 when she became queen? If Mr. Peanut has sounded familiar to you in Planters' recent commercials, there's a good reason for that: the ads are voiced by none other than actor Bill Hader, of SNL fame and Barry acclaim. And for more surprising celebrity roles, check out The 30 Funniest Celebrity Commercials. The Humane Society of California has filed a complaint against the ASPCA with the Attorney General. Why don't libraries smell like bookstores? He is known for his work on American Sniper (2014), Ancient Aliens (2009) and The Curse of Oak Island (2014). From rescue to recovery to adoption, the ASPCA is there for animals every step of the way. Who does the voice over for aspca tv commercial. Allison Janney's character in I, Tonya, may have primarily shrieked foul-mouthed commands at her on-screen daughter, but in real life, the veteran actress knows how to turn on the charm. American Society for the Prevention of Cruelty to Animals receives 85.60 out of 100 for their Charity Navigator rating. In fact, it was because of Arnett's work on the GMC commercials that he lost out on the role of talking car, K.I.T.T., in the 2008 TV movie Knight Rider, a part that ended up going to Val Kilmer instead. However, his most recognizable voice-over role is for Dunkin' Donuts' "America Runs on Dunkin'" campaign, for which he's been providing voice work since 2007. And for more celebrity fun, discover the 30 Most Powerful Celebrity Siblings. The Last Man Standing star has been voicing the travel initiative's TV and radio commercials since they first hit the air in 2009. Someone suggested Mira Sorvino, and now all I can see is Romy White. John Goodman has been doing voice-over work for animated movies and TV shows for years, working on everything from Futurama to Monsters, Inc. to The Princess and the Frog. If you've ever been eager to get a pat on the back for safe driving from a celebrity, Nationwide Insurance has got you covered. Does pumpkin pie need to be refrigerated? Oscar winner Matt Damon may be best known for his work as an action star, but he's also been earning a major payday as the voice of TD Ameritrade since 2012, when he took over for Grace & Frankie star Sam Waterston. If you think that's funny, you'll love The 30 Funniest Things Celebrities Have Said About Marriage. However, it's not just newcomers to the industry who keep the lights on with commercial work. Paul Rudd's easy charm has made him a box office draw for decades in films like Anchorman and Knocked Up, and apparently, a big hit in the ad world, as well. John Corbett's southern charm made a fan favorite on Sex and the City, and, more recently, the actor has lent his West Virginia accent to commercials for Applebee's. If you've ever wondered why you've felt a sudden hankering for episodes of Living Single and Pizza Hut at the same time, the reason is obvious: rapper/actress Queen Latifah was the voice behind the pizza chain's commercials for years. In 2013, Paul lent his voice to Cadillac's Summer's Best Event, advertising the company's ATS line of vehicles. In 2010 the ASPCA (The American Society for the Prevention of Cruelty to Animals) came out with a commercial that would shock the advertisement industry. However, that's not Corbett's only recognizable voice-over role: he's also been one of the voices of Walgreens since 2012. 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2020 aspca commercial narrator 2020


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Canada 3000 (Airport Authorities): Successful appeal to the Supreme Court of Canada
Frank J.C. Newbould, Q.C. (Counsel)
Frank has earned a reputation as a "giant" in commercial law from his career spent as a judge, counsel and arbitrator.
Frank spent more than 10 years as a judge of the Ontario Superior Court of Justice, including most recently as Team Leader of the Commercial List in Toronto, the country's first and busiest commercial court. Cases he heard included domestic and cross-border insolvency matters, corporate amalgamations and reorganizations, proceedings for relief under business corporation statutes including oppression actions, and other complex commercial matters and disputes. Among his numerous high profile cases, Justice Newbould conducted the first cross-border joint trial in Canada with the Delaware Bankruptcy Court in the global proceedings involving the Nortel Networks group of companies to determine entitlement to US$7.3 billion in proceeds of sale, using state-of-the-art technology.
Prior to his appointment to the bench, he acted as litigation counsel in many large and complex commercial matters, including appearing 18 times at the Supreme Court of Canada. He has been recognized in all major professional directories including Chambers Global, the International Who's Who of Business Lawyers and the Lexpert / American Lawyer Guide to the 500 Leading Lawyers in Canada. In 2016, Canadian Lawyer magazine named him one of the Top 25 Most Influential Lawyers in Canada.
Frank is a
Fellow of the American College of Trial Lawyers
Chartered Arbitrator with the ADR Institute of Canada
Member of the ICC Canada Arbitration Committee
Queen's Counsel (1981)
Past Director of the Advocate's Society
Past President of the Lawyers' Club of Toronto
Frank J.C. Newbould, Q.C. will be speaking at the 10th Annual Turnaround Management Association Brazil conference on the topic "International Co-ordination of Insolvency Proceedings" in São Paulo, Brazil.
Frank J.C. Newbould, Q.C. will be chairing a panel at the International Insolvency Institute (III) annual conference in New York on the topic "Court to Court Communication in Cross-border Insolvencies."
Frank J.C. Newbould, QC is speaking on a panel at the International Association of Defense Counsel's 2018 Annual Meeting in Lisbon, Portugal entitled "Help, My Bankruptcy is Getting International" regarding cross-border insolvency.
Frank J.C. Newbould, Q.C is the keynote speaker at The Advocates' Society conference called "Insolvency Litigation."
Frank J.C. Newbould, Q.C is speaking on a panel at the 2018 Regional INSOL conference in New York City regarding Chapter 15 Recognition Proceedings and the public policy exception to recognition from a Canadian perspective.
Frank J.C. Newbould, Q.C is speaking on a panel at The Advocates' Society conference "Examining and Cross-Examining Experts" on the topic of "Practical Tips for Preparing and Examining an Expert Witness in Chief."
Frank J.C. Newbould, Q.C. will be the keynote speaker at the International Insolvency Institute (III) Regional Conference in Mexico City on the topic of "International Insolvency and Arbitration as a Legal Vehicle to Settle an Insolvency."
Frank Newbould, Q.C., will be speaking on the topics of ethical issues in interviewing prospective arbitrators and how to deal with difficult counsel at The Advocates' Society Continuing Professional Development program "Arbitration Advocacy."
Frank Newbould, Q.C., will be giving two lectures at the Peter A. Allard School of Law at the University of British Columbia, on cross-border insolvency litigation and on corporate finance.
TGF is pleased to announce that the Honourable Frank Newbould, Q.C. has joined as Counsel to the firm.
Q&A with Frank Newbould, Q.C.
LL.B (University of Toronto) 1967
B.A. (Honours – Math and Economics) (Queen's University) 1964

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HOMEFebruary 02, 2023
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(c) To Protect the Rights of the Company and Others. To the fullest extent permitted by applicable law, we may also disclose your information (including Personal Information) if we believe in good faith that doing so is necessary or appropriate to: (i) protect or defend the rights, safety or property of OFS Energy Fund or third parties (including through the enforcement of this Privacy Policy, our Terms of Use, and other applicable agreements and policies); or (ii) comply with legal and regulatory obligations (e.g., pursuant to law enforcement inquiries, subpoenas or court orders). To the fullest extent permitted by applicable law, we have complete discretion in electing to make or not make such disclosures, and to contest or not contest requests for such disclosures, all without notice to you.
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The Site may contain content that is supplied by a third party, and those third parties may collect Usage Information and your Device Identifier when pages from the Site are served to you. In addition, when you are on the Site you may be directed to other services that are operated and controlled by third parties that we do not control. We are not responsible for the data collection and privacy practices employed by any of these third parties or their services and they may be tracking you across multiple sites and may be sharing the results of that tracking with us and/or others. For example, if you "click" on a link, the "click" may take you off the Site onto a different site. These other sites may associate their Tracking Technologies with you, independently collect data about you, including Personal Information, and may or may not have their own published privacy policies. We encourage you to note when you leave the Site and to review the third-party privacy policies of all third-party websites and exercise caution in connection with them.
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Information Management | TOKYO OHKA KOGYO CO., LTD.
as one of our most important management issues.
Aiming to become a company that can earn the trust of all stakeholders, we are continuously working to manage and maintain information security and appropriately protect our exclusive information as well as externally obtained information including personal information.
across the Group, including overseas affiliates and subsidiaries.
The Committee works to strengthen the information management systems of the entire Group.
During the fiscal year under review, information management committees were set up at key subsidiaries, putting into place a system for collaborating organizationally under the guidance of TOK's Information Management Committee.
The Tokyo Ohka Kogyo Group (Tokyo Ohka Kogyo Co., Ltd. and its subsidiaries; hereinafter referred to as the "TOK Group") has positioned managing risks related to information assets as an important business issue and is working to implement various measures in line with the following policy in order to fulfill its corporate social responsibility.
(1) The TOK Group shall comply with laws and regulations related to information security, social norms, in-house rules, etc.; appropriately protect all information assets it possesses, including business information, customer and sales information, personal information, and technical information; and use those information assets only for stated purposes and by those with the stipulated authority in order to effectively conduct operations.
(2) The TOK Group will develop and maintain communication tools and security infrastructure to a reasonable extent so that information assets can be effectively utilized.
(3) The TOK Group shall establish an Information Management Committee and create, maintain, and promote an information asset management system throughout the Group.
(4) The TOK Group shall properly manage information assets it possesses through various measures including human, physical, and system ones and IT in order to prevent the leak, unauthorized alteration, theft, destruction, etc., of those assets.
(5) The TOK Group shall regularly and continually conduct in-house training and work to raise awareness and educate employees about in-house rules, etc.
(6) If an information security related incident or similar event occurs, the TOK Group shall work to minimize damage and take steps to prevent a reoccurrence.
(7) The TOK Group shall regularly conduct audits and continually implement improvements as part of its information asset management.
Appendix: This Policy shall be established and revised through the drafting by the Information Management Committee.


The Staff of the Securities and Exchange Commission's Division of Corporation Finance recently published a number of new interpretive positions that are significant to public companies. This Client Alert discusses these interpretations and provides links to the relevant documents.
The Division's Financial Reporting Manual is extremely useful for finding the Staff's views on common accounting issues and related disclosure. The new update (which is dated as of March 31, 2011) includes a number of technical updates, but also includes significant new information with regard to subsidiary guarantor financial statements, internal control over financial reporting requirements for newly public companies, and reporting requirements in a reverse recapitalization. As the Staff has begun updating the Financial Reporting Manual much more frequently, it is now providing a summary of changes at the beginning of the manual.
The Staff revised its guidance regarding Item 401 of Regulation S-K relating to disclosure on non-continuing directors. Under new C&DI Question 116.10, if a company provides its Form 10-K Part III information by incorporation by reference from its proxy statement, it need not include information regarding non-continuing directors. Importantly, however, the Staff did not change its view with regard to the inclusion of the Part III information directly in the Form 10-K from that expressed in the withdrawn C&DI Question 116.08. As such, if a company includes this information directly in the Form 10-K itself (either by choice or because it did not file a proxy statement containing the Part III information within 120 days of fiscal year end), it must provide information about non-continuing directors in its Form 10-K.
The Staff issued new interpretations related to Form 12b-25, disclosure regarding "say-on-frequency" votes, executive compensation disclosure, and non-GAAP financial measures. Clicking on each title below will direct you to each new C&DI.
This new C&DI addresses the situation where a company needs to file a Form 12b-25 to provide notice of a late periodic filing, but does not believe that it will be able to file the periodic report within the applicable extension period provided by Rule 12b-25(b). This presents an issue, as there is a box in Part II of the Form that requires the company to indicate that it will file by the extended deadline. Under the C&DI, the Staff makes clear that the company should not check that box if it does not intend to file by the extended deadline. The significant part of the new C&DI is the statement that the Commission will consider a filing made by the extended deadline to be timely, even where the company did not check the box in Part II.
This new C&DI addresses the disclosure related to "say-on-frequency" votes. The Staff indicates that, with respect to "say-on-frequency" votes, a company is not required to disclose the number of broker non-votes; rather, the company is required to disclose the number of votes cast for each of the one-, two- or three-year frequency options and the number of abstentions.
if a company disclosed the initial "say-on-frequency" voting results in a Form 8-K, the board's subsequent decision as to how frequently to hold the "say-on-pay" vote must be disclosed in an amendment to the original Form 8-K (i.e., it should not be filed as a new Form 8-K).
This new C&DI provides that a company may omit disclosure regarding disability plans that do not discriminate in scope, terms or operation, in favor of its executive officers or directors, and that are available generally to all salaried employees. This C&DI places disability plans in the same category as group life, health, hospitalization, and medical reimbursement plans.
This new C&DI states that Regulation G and Item 10(e) of Regulation S-K apply to any non-GAAP financial disclosures, other than target level disclosures (e.g., financial performance targets) contained in the Compensation Discussion and Analysis, that are included in a company's proxy statement. It is important to note the language in this C&DI regarding the means of providing the required GAAP reconciliations. Specifically, it indicates that the Staff will not object if a company includes these reconciliations in a prominently cross-referenced annex or by incorporation by reference to the relevant pages of the company's Form 10-K containing such reconciliation. The Division repeated this guidance in Question 108.01 in the C&DIs on Non-GAAP Financial Measures.
This new C&DI expresses the Staff's view that the grant date fair value for stock and option awards that are subject to performance conditions must be reported based on the probable outcome of the performance conditions as of the grant date, even if the actual outcome is known as of the disclosure date.
The Division released a statement outlining its analysis for determining whether to grant an "ineligible issuer" waiver to a company that has lost its status as well-known seasoned issuer for having violated the anti-fraud provisions of the federal securities laws. Under Securities Act Rule 405, the Commission may grant waivers of "ineligible issuers" status upon a showing of good cause. The Commission has delegated the authority to grant such waivers to the Director of the Division. The statement sets forth the analysis that the Division will evaluate in determining the appropriateness of granting a waiver. The Division also published three recent no-action letters that apply this analysis -- Raymond James Financial, Inc., JPMorgan Chase & Co., and Regions Financial Corporation.


text:
History! New York Legalizes Gay Marriage
ALBANY, N.Y. — New York lawmakers narrowly voted to legalize same-sex marriage Friday, handing activists a breakthrough victory in the state where the gay rights movement was born.
New York will become the sixth state where gay couples can wed and the biggest by far.
LINK: Obama Believes Gay Marriage "Best Addressed By States"
LINK: Super Bowl Hero: "Gay Marriage Will Lead To Anarchy"
LINK: Gay Black Men: How They Overlook The Women Who Love Them
"We are leaders and we join other proud states that recognize our families and the battle will now go on in other states," said Sen. Thomas Duane, a Democrat.
Gay rights advocates are hoping the vote will galvanize the movement around the country and help it regain momentum after an almost identical bill was defeated here in 2009 and similar measures failed in 2010 in New Jersey and this year in Maryland and Rhode Island.
Though New York is a relative latecomer in allowing gay marriage, it is considered an important prize for advocates, given the state's size and New York City's international stature and its role as the birthplace of the gay rights movement, which is considered to have started with the Stonewall riots in Greenwich Village in 1969.
The New York bill cleared the Republican-controlled state Senate on a 33-29 vote. The Democrat-led Assembly, which passed a different version last week, is expected to pass the new version with stronger religious exemptions and Democratic Gov. Andrew Cuomo, who campaigned on the issue last year, has promised to sign it. Same-sex couples can begin marrying begin 30 days after that.
The passage of New York's legislation was made possible by two Republican senators who had been undecided.
Sen. Stephen Saland voted against a similar bill in 2009, helping kill the measure and dealing a blow to the national gay rights movement.
"While I understand that my vote will disappoint many, I also know my vote is a vote of conscience," Saland said in a statement to The Associated Press before the vote. "I am doing the right thing in voting to support marriage equality."
Gay couples in gallery wept during Saland's speech.
(See: Senate blocks bill that included ethanol repeal)
Sen. Mark Grisanti, a GOP freshman from Buffalo, also said he would vote for the bill. Grisanti said he could not deny anyone what he called basic rights.
The effects of the law could be felt well beyond New York: Unlike Massachusetts, which pioneered gay marriage in 2004, New York has no residency requirement for obtaining a marriage license, meaning the state could become a magnet for gay couples across the country who want to have a wedding in Central Park, the Hamptons, the romantic Hudson Valley or that honeymoon hot spot of yore, Niagara Falls.
New York, the nation's third most populous state, will join Connecticut, Iowa, Massachusetts, New Hampshire, Vermont and Washington, D.C., in allowing same-sex couples to wed.
For five months in 2008, gay marriage was legal in California, the biggest state in population, and 18,000 same-sex couples rushed to tie the knot there before voters overturned the state Supreme Court ruling that allowed the practice. The constitutionality of California's ban is now before a federal appeals court.
While court challenges in New York are all but certain, the state – unlike California – makes it difficult for the voters to repeal laws at the ballot box. Changing the law would require a constitutional convention, a long, drawn-out process.
The sticking point over the past few days: Republican demands for stronger legal protections for religious groups that fear they will be hit with discrimination lawsuits if they refuse to allow their facilities to be used for gay weddings.
The climactic vote came after more than a week of stop-and-start negotiations, rumors, closed-door meetings and frustration on the part of advocates. Online discussions took on a nasty turn with insults and vulgarities peppering the screens of opponents and supporters alike and security was beefed up in the capitol to give senators easier passage to and from their conference room.
The night before, President Barack Obama encouraged lawmakers to support gay rights during a fundraiser with New York City's gay community. The vote also is sure to charge up annual gay pride events this weekend, culminating with parades Sunday in New York City, San Francisco and other cities.
Despite New York City's liberal Democratic politics and large and vocal gay community, previous efforts to legalize same-sex marriage failed over the past several years, in part because the rest of the state is more conservative than the city.
The bill's success this time reflected the powerful support of Cuomo and perhaps a change in public attitudes. Opinion polls for the first time are showing majority support for same-sex marriage, and Congress recently repealed the "don't ask, don't tell" policy that barred gays from serving openly in the military.
In the week leading up to the vote in New York, some Republicans who opposed the bill in 2009 came forward to say they were supporting it for reasons of conscience and a duty to ensure civil rights.
Pressure to vote for gay marriage also came from celebrities, athletes and New York City Mayor Michael Bloomberg, the Republican-turned-independent who has long used his own fortune to help bankroll GOP campaigns and who personally lobbied some undecided lawmakers. Lady Gaga has been urging her 11 million Twitter followers to call New York senators in support of the bill.
While the support of the Assembly was never in doubt, it took days of furious deal-making to secure two Republican votes needed for passage in the closely divided Senate.
Representatives of the Roman Catholic Church, Orthodox rabbis and other conservative religious leaders fought the measure, and their GOP allies pressed hard for stronger legal protections for religious organizations.
Each side of the debate was funded by more than $1 million from national and state advocates who waged media blitzes and promised campaign cash for lawmakers who sided with them.
But GOP senators said it was Cuomo's passionate appeals in the governor's mansion on Monday night and in closed-door, individual meetings that were perhaps most persuasive.
The bill makes New York only the third state, after Vermont and New Hampshire, to legalize marriage through a legislative act and without being forced to do so by a court.
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Lil' Kim & Nicki Minaj To Perform Together At BET Awards?
Sean Kingston Released From The Hospital!
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Gay Marriage	, New York	, News
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20 Tweets Dragging Roseanne Barr To A White Privilege Hell


text:
\section{Introduction}

It is a standard paradigm of modern astrophysics that the majority of
galaxies -- possibly with the exception of very low mass galaxies and/or dwarf
irregulars -- contains massive black holes (MBHs) at their centres (see,
e.g., \cite{Gultekin:2009fk} and references therein). Over the past two
decades, mainly thanks to studies with the Hubble Space Telescope and
high-angular resolution observations with Adaptive Optics at major
ground-based telescopes, we have also learned that the majority of
galaxies contains so-called {\it nuclear star clusters} (NSCs) at their
photometric and dynamical centres. These clusters are the densest and
most massive clusters that can be found in the present-day
Universe. They have masses between a few $10^{5}$ to
$10^{8}$\,M$_{\odot}$ and half light radii of a few to a few tens of
parsecs. NSCs do not consist of single-age stellar populations, but
rather show signs of repeated star formation along their host
galaxies' lifetime, i.e.\ they are in their properties significantly
different from globular clusters. Most intriguingly, NSCs have been
found to coexist with massive black holes (for the properties of NSCs,
see \cite{Boker:2010ys,Georgiev:2014ve,Georgiev:2016nr} and references therein).

The evolution of a star cluster containing an MBH is a decades-old
problem of stellar dynamics that has been studied by a large number of
authors with a wide range of techniques (analytical, Fokker-Planck,
Nbody). Peebles (1972) \cite{Peebles:1972fk} proved that, while the
statistical thermal equilibrium must be violated close to a MBH in a
galactic nucleus due to tidal disruptions, stellar collisions and
gravitational captures, there exists a steady state with net inward
flux of stars.  This is a quasi-steady state solution,
where the stellar density takes a power-law form
$\rho \propto r^{-\gamma}$. This finding was corroborated for a
single-mass population by Bahcall and Wolf \cite{Bahcall:1976vn} and
subsequently for multi-mass stellar populations with realistic number
fractions (e.g.,
\cite{Bahcall:1977ys,Lightman:1977ly,Murphy:1991zr,Amaro-Seoane:2004kx,Alexander:2005fk,Merritt:2006ys,Alexander:2009gd,Amaro-Seoane:2011qv}
and references therein). This so-called stellar density {\it cusp}
will be fully developed after a so-called {\it relaxation time}, the
time necessary for the randomisation of the cluster phase space via
close encounters between stars (so-called two-body relaxation), which
is typically below a Hubble time for a NSC in a Milky Way-like galaxy
For a cluster composed only of stars of a single mass the predicted
value is $\gamma=1.75$. For realistic, multi-mass clusters, the lower
mass stars have $\gamma=1.5$, while the heavier stars (and in
particular stellar mass black holes) will follow a steeper
distribution ($\gamma_{BH}\approx2$; see
\cite{Alexander:2009gd,Amaro-Seoane:2011qv}). The cusp will be well
developed inside the radius of influence of the MBH, which is roughly
the radius of a sphere that contains once to twice the black hole mass
in form of stars (or stellar remnants) \cite{Alexander:2005fk}.

Although stellar cusps around MBHs are a robust theoretical
prediction, they have been rather elusive observationally. That is
mainly because of the great distances of MBHs: Their radii of
influence are often resolved only by a few pixels in imaging or
spectroscopy, which means that a handful of rare bright stars can bias
the measured cluster structure significantly, as can be seen very well
in the case of our own Milky Way (see discussion in
\cite{Schodel:2007tw}). When comparing theoretical predictions with
observations in nature, it is also important to be aware that
theoretical models are often highly simplified, e.g.\ they typically
are setup with clusters of a single age stellar population, and do not
suffer from observational effects such as strong and spatially
variable interstellar extinction.

\begin{figure}[htb]
\label{Fig:overview}
\includegraphics[width=\textwidth]{fig1.pdf}
\caption{A progressive zoom into the Galactic Center. Left: Spitzer
  $4.5\,\mu$m image \cite{Stolovy:2006fk} of the central
  $100\,\mathrm{pc}\times100\,\mathrm{pc}$ of the Galaxy. Coordinates
  are given as offsets from the MBH Sgr\,A*. The NSC is the
  bright, compact structure in the centre of the image. Middle:
  NACO/VLT $2.2\,\mu$m image of the central
  $3\,\mathrm{pc}\times3\,\mathrm{pc}$ around Sgr\,A*. Right: NACO/VLT
  $2.2\,\mu$m image of the central $1.6"\times1.6"$
  ($0.06\,\mathrm{pc}\times0.06\,\mathrm{pc}$) around Sgr\,A*. Stellar
  orbits determined by \cite{Gillessen:2016uq} are over-plotted onto
  the image. Sgr\,A* is visible as a near-infrared source at the image
centre.}
\end{figure}

The best case for testing the stellar cusp hypothesis is the centre of
the Milky Way. In the Galactic Centre (GC), an MBH of about
$4\times10^{6}$\,M$_{\odot}$, called Sagittarius\,A* (Sgr\,A*), is
surrounded by an NSC of about $2.5\times10^{7}$\,M$_{\odot}$, at a
distance of $\sim$8\,kpc (\cite{Genzel:2010fk,Boehle:2016zr,
  Gillessen:2016uq,Schodel:2014fk} and references therein). With high
angular resolution observations we can therefore probe the cluster
structure and dynamics on scales of milli-parsecs, which means that
the GC is a prime laboratory for studying the interaction of a stellar
cluster with an MBH \cite{Schodel:2014bn}. Figure\,\ref{Fig:overview}
provides an overview of the GC and a progressive zoom toward the MBH
Sagittarius\,A* (Sgr\,A*).

It is important to keep in mind the limitations on observational
studies of the GC: (1) Due to the extremely high interstellar
extinction, stars can only be detected with reasonable sensitivity in
the near-infrared. In this region, however, intrinsic stellar colours
are small and in combination with the strong differential reddening
caused by the small-scale variability of extinction it is therefore
very hard to classify the stars. For example, it is not trivial to
distinguish between an old, cold giant star and a young, hot massive
star by means of imaging and stellar colours. (2) Due to the extreme
density of the NSC, one needs to work with high angular resolution,
typically at the diffraction limit of ground-based 8-10m-class
telescopes, which can only be achieved with special techniques
(Adaptive Optics and speckle imaging). Even then, most faint stars
(main sequence stars of less than two solar masses) cannot be detected
because of the source crowding. Hence, we can only observe the tip of
the iceberg, on the order a few to 10\% of all the stars suspected to
exist at the GC.

Because of the observational limitations, evidence on the existence of
a stellar cusp at the GC was elusive. Although the detection of a cusp
was claimed by first high angular resolution observations
\cite{Schodel:2007tw,Genzel:2003it}, the actual situation turned out
to be more complex. Only stars older than the cluster relaxation time
can serve as suitable tracers of a cusp, but there are many massive
young stars present in the central parsec around Sgr\,A*. These are
too young to be dynamically relaxed. Once the pollution from young
stars was taken into account, it appeared that the stellar surface
number density within a few 0.1\,pc of the MBH at the GC was close to
flat, or even decreasing
\cite{Buchholz:2009fk,Do:2009tg,Bartko:2010fk}. The lack of late-type
giants close to the MBH had been reported before (see, e.g.,
discussion fo this topic in the review by \cite{Genzel:2010fk}), but
these more detailed studies were now considered to be incompatible
with the existence of a stellar cusp. This is the origin of the {\it
  missing cusp problem}.

The existence or not of a stellar cusp around the MBH at the GC has
implications for other galaxies as well, assuming that the Milky
Way's centre is representative for the nuclei of normal galaxies. Observational
confirmation or rejection of a stellar cusp would not only have
fundamental importance for our understanding of stellar
dynamics. It is also of particular importance for gravitational wave
astronomy. So called Extreme Mass Ratio Inspirals (EMRIs) are
considered the most exquisite probes of General Relativity and of the
related astrophysics of stellar remnant plus MBH systems
\cite{Amaro-Seoane:2007ve}. The possibility of observing EMRIs with
future gravitational wave observatories in space, such as LISA (Laser Interferometer Space Antenna )
\cite{Amaro-Seoane:2012ys,Amaro-Seoane:2013zr} or Taiji
\cite{Gong:2015zr} is directly linked to the question whether stellar
cusps exist around MBHs or not
\cite{Hopman:2005dn,Amaro-Seoane:2011qv}.

Motivated by the fundamental importance of this topic, we have
recently undertaken new observational and theoretical
studies. Observationally, we pushed the detection limit to fainter
stars. The observations were then compared to new, more realistic
Nbody simulations. We have found that a stellar cusp does indeed exist
at the GC and that its properties agree with our expectations. The
details of our work can be consulted in these three papers:
1. Gallego-Cano et al. (submitted to A\&A, arXiv:1701.03816);
2. Sch{\"o}del et al.  (submitted to A\&A, arXiv:1701.03817);
3. Baumgardt et al.  (submitted to A\&A, arXiv:1701.03818).  We
will briefly describe our findings in the following sections.

\section{Surface density of stars around the MBH Sgr\,A*}

\begin{figure}[htb]
\label{Fig:LF}
\includegraphics[width=\textwidth]{fig2.pdf}
\caption{Properties of the observable stellar population at the
  GC. {\it Left}: Simple population synthesis model of the GC stellar
  population, assuming continuous star formation, modified from
  Fig.\,16 in \cite{Schodel:2007tw} (Reproduced with permission from
  Astronomy \& Astrophysics, \copyright ESO). The distance modulus and
  extinction were added to the stellar magnitudes, which means that
  the magnitude values on the x-axis correspond to observed
  values. The upper panel shows the mean mass of all stars and of old
  stars (lifetime $> 1$\,Gyr) only. The middle panel shows a
  luminosity function. The lower panel displays the fraction of old
  stars in each magnitude interval. The completeness limit due to
  source crowding of previous studies was limited to
  $K_{s}\lesssim17.5$, while the sensitivity limit of spectroscopic
  studies is $K_{s}\approx16$. At $K_{s}<17.5$, number counts of old
  stars in the GC will therefore be dominated by horizontal branch/red
  clump (HB/RC) stars, core-helium burning giants. {\it Right}:
  $K_{s}$ luminosity function of stars within a projected distance of
  $R\lesssim10"$ of Sgr\,A*, extracted from a deep NACO/VLT S13 image.
  The bump centred at $K_{s}\approx15.75$ corresponds to the RC. The
  sharp drop in detected stars at $K_{s}>18$ is due to extreme source
  crowding, which impedes the detection of fainter stars. While RC
  stars and brighter giants have dominated the stellar density
  measurements of all previous work, we use measurements of resolved
  and unresolved stars at $Ks\gtrsim17.5$ in our new work.}
\end{figure}

Before interpreting the stellar surface and light densities, it is
important to have an approximate understanding of the stellar
population we expect to observe at the GC. While we are still far from
having a detailed understanding of the stellar population and its
formation history in the inner few parsecs of the Milky Way, the
following assumptions appear to be robust, according to our current
best knowledge: The NSC has undergone repeated star formation
episodes throughout its lifetime, with the most recent events
occurring a few $10^{6}$ and a few 10\,Myr ago. The majority of the
stars are old, with an estimated 80\% having formed more than 5\,Gyr
ago \cite{Genzel:2010fk,Pfuhl:2011uq}.

The left panel in Fig.\,\ref{Fig:LF} shows a simple model of the
stellar population of the NSC
assuming a continuous star formation history (taken from Fig.\,16 in
\cite{Schodel:2007tw}). As mentioned above, it is very hard to
classify stars at the GC because photometric studies do usually not
cover a sufficient wavelength range and are usually not accurate and
precise enough to break the degeneracy between intrinsic stellar
colours and interstellar reddening and because spectroscopic studies
are extremely time-consuming and limited to the brightest
stars. Therefore, the diagram in the left panel in Fig.\,\ref{Fig:LF} is
valuable because it can give us an approximate idea of the ages and
masses of stars of a given observed brightness at the GC. If we are
interested in identifying a stellar cusp, then it is important to
focus on stars that are at least a few Gyr old. We can do this by selecting
spectroscopically classified stars and/or by limiting the brightness
range of the tracer population.  Previous studies of the NSC structure
(\cite{Buchholz:2009fk,Do:2009tg,Bartko:2010fk}) were dominated by
stars of K-band magnitudes brighter than $\sim$17.5, in particular by
Red Clump (RC) stars, helium core burning giants with observed K-band
magnitudes $15-16$ at the distance and extinction of the GC.

RC stars are a convenient tracer population because they are, on
average, a few Gyr old. We can also see in the left panel in
Fig.\,\ref{Fig:LF} that stars of K-magnitudes 18 or fainter would also
be suitable tracer populations because they have low mean masses and
are therefore probably, on average, at least a few Gyr old.

In our new work, we focused explicitly on this faint, old, low mass
stellar population. We used K-band high angular resolution
observations from the camera NACO at the ESO VLT 8m telescope. Several
epochs of high quality images were stacked in order to increase the
sensitivity. Subsequently, correction factors for stellar crowding and
interstellar extinction were determined and applied to the
data. Systematic effects arising from different choices of key
parameters in the software packages that identify the stars in images
were explored. Finally, the stellar surface densities were determined
as a function of distance from the central MBH. Spherical symmetry of
the cluster was assumed, which is not strictly correct, but accurate
on a 10-20\% level. In parallel, we also explored the diffuse light
density from unresolved stars that could be measured in the images
after subtracting all identified, resolved stars and the emission from
diffuse, ionised gas.

In order to constrain the structure of the entire NSC and to be able
to deproject the observed quantities, these data were complemented, at
projected distances $R\gtrsim1$\,pc from Sgr\,A*, by star
density/surface brightness measurements from other sources, with lower
angular resolution and/or sensitivity, but taken over a larger field
(\cite{Schodel:2014fk,Fritz:2016fj}). The latter were scaled to our
data in the overlapping regions. In Fig.\,\ref{Sigmanuker} we show the
surface brightness from unresolved stars from 0.01\,pc to 20\,pc as
well as the star counts for faint resolved stars (K-magnitudes
$\sim$18) and RC stars (K-magnitudes $\sim$15-16). The diffuse
flux from the unresolved stars traces sub-giants and main sequence
stars of K-band magnitude $19-20$, which have masses of about
$0.8-1.8$\,M$_{\odot}$. All these three tracer populations have
similar masses and can be old enough to be dynamically relaxed.

\section{Properties of the stellar cusp at the GC}

As Fig.\,\ref{Sigmanuker} shows, the three studied tracer populations
show a very similar distribution. The projected densities can all be
approximated well by single power-laws at projected distances $R<1$\,pc. Only
the brightest population, the red clump giants, show some systematic
deviations at around $R=0.2$\,pc and a possible decline at
$R<0.05$\,pc. The red line in Fig.\,\ref{Sigmanuker} indicates a fit
with a {\it Nuker} law \cite{Lauer:1995fk}:

\begin{figure}[htb]
\label{Sigmanuker}
\includegraphics[width=\textwidth]{fig3.pdf}
\caption{Surface light/stellar number density at the GC plotted
  against the projected distance from Sgr\,A*. The black line is the
  surface light density from the unresolved stars (Sch{\"o}del et al.,
  submitted to A\&A,  arXiv:1701.03817). In order to constrain the shape of the NSC at
  distances $> 2$\,pc, we used the data from \cite{Fritz:2016fj} and
  scaled them in the overlap region to our data. A constant flux of
  6.4\,mJy\,arcsec$^{-2}$ was subtracted to remove the contamination
  by the surrounding nuclear bulge and Galactic bar, which can be
  approximated by a constant on these scales.  The red line is a
  best-fit Nuker model. The blue and green lines are scaled stellar
  number densities from Gallego-Cano et al. (submitted to A\&A, arXiv:1701.03816) for RC
  giants and faint subgiants/main sequence stars. }
\end{figure}

\begin{equation}
\rho(r) = \rho(r_{b})2^{(\beta-\gamma)/\alpha}\left(\frac{r}{r_{b}}\right)^{-\gamma}\left[1+\left(\frac{r}{r_{b}}\right)^{\alpha}\right]^{(\gamma-\beta)/\alpha},
\end{equation}

where $r$ is the 3D distance from the central MBH, $r_{b}$ is the
break radius, $\rho$ is the 3D density, $\gamma$ is the exponent of
the inner and $\beta$ the one of the outer power-law, and $\alpha$
defines the sharpness of the transition.  We carried out fits with
different parameters (e.g., for the value of $\alpha$ that was kept
fixed at a value of 10 during the fits) and data (data at large $R$ from
\cite{Schodel:2014fk} or \cite{Fritz:2016fj}) and determined mean
parameters and uncertainties from the resulting best-fit parameters of
the different tries (the formal uncertainties were always very
small). We obtain, for the unresolved stellar light
$r_{b,diffuse} = 3.2\pm0.2$\,pc, $\gamma_{diffuse}=1.16\pm0.02$,
$\beta_{diffuse}=3.2\pm0.3$, and
$\rho_{diffuse} (r_{b})=0.67\pm0.05$\,mJy\,arcsec$^{-3}$, for the star
counts of faint, resolved stars $r_{b,faint}=3.0 \pm 0.4$ pc
($77 \pm 10"$), $\gamma_{faint} = 1.29 \pm 0.02$,
$\beta_{faint} = 2.1 \pm 0.1$, and a density at the break radius of
$\rho_{faint} (r_{b})=3900 \pm 900$\,pc$^{-3}$, and for the RC stars
$r_{b,RC}=3.4 \pm 0.5$ pc ($110 \pm 13"$),
$\gamma_{RC} = 1.28 \pm 0.07$, $\beta_{RC} = 2.26 \pm 0.04$, and
$\rho_{RC} (r_{b})=1700 \pm 500$\,pc$^{-3}$.

We cannot directly compare the values of the normalisation parameters
$\rho$. As concerns $\beta$, it is not very well constrained. On the
other hand, the break radius $r_{b}$ is well constrained around 3\,pc
and the inner power-law index $\gamma$ as well. The break radius
corresponds roughly to the radius of influence of the Sgr\,A*, i.e.\ the
radius inside which we expect the stellar cusp to appear
\cite{Alexander:2005fk}. Both the stellar number and light densities
may suffer from not well constrained systematic biases (uncertainties
in sky background subtraction or completeness corrections etc.). If we
adopt conservative values from averaging the three values, we obtain
$r_{b}=3.2\pm0.2$ and $\gamma=1.24\pm0.07$, taking the standard
deviations as uncertainties. Obviously, the stellar density displays a
cusp and a core-like (flat) density law can be excluded with very high
confidence.

\section{Discussion and conclusions}

We find that the stars at the GC follow a cusp-like density
distribution inside the radius of influence of the central MBH. Our
findings resolve the ambiguity from previous work. The cusp is less
steep than what is expected for a single age population that is older
than the relaxation time. In the latter case one would expect to
observe a so-called Bahcall-Wolf cusp with $\gamma\geq1.5$. Numerical
experiments were performed by Baumgardt et
al. (arXiv:1701.03818) to interpret our data. They performed Nbody simulations of a more
realistic NSC, assuming repeated star formation episodes every
1\,Gyr. This means that most stars will not have had the time to fully
relax dynamically, which will flatten the cusp. The results of the
simulations agree very well with the data.

There appears to be a lack of giant stars at small projected distances
of $R\lesssim0.1$\,pc from Sagittarius\,A*. The missing few dozens of
giants could be explained if their envelopes were removed in the past,
thus rendering them invisible to observations. While collisions between
stars or between stellar remnants and stars are probably not effective
enough, collisions with high-density clumps in a formerly existing
star-forming gas disc around Sagittarius\,A* provide a viable
mechanism \cite{Amaro-Seoane:2014fk}. We know that such a disc must
have existed in the past because of the presence of many young,
massive stars in this region that move in a coherent, disc-like
pattern (e.g., (e.g.,
\cite{Beloborodov:2006ff,Lu:2009bl,Genzel:2010fk}).

We conclude that a stellar cusp exists around Sagittarius\,A* and that
its properties agree with what we expect theoretically. Densities in
excess of a few $10^{7}$\,M$_{\odot}$\,pc$^{-3}$ are reached at
distances $r<0.01$\,pc from the central black hole (Sch\"odel et al.,
submitted to A\&A, arXiv:1701.03817).  This has significant
implications for gravitational wave astronomy. The existence of a
stellar cusp in the Milky Way implies the existence of such structures
in other galaxies with similar or smaller MBHs. Therefore we can
expect to observe significant numbers of EMRIs with future space-based
gravitational wave observatories
\cite{Hopman:2005dn,Amaro-Seoane:2012ty,Amaro-Seoane:2012ys,Amaro-Seoane:2013zr}.

\ack

The research leading to these results has received funding from the
European Research Council under the European Union's Seventh Framework
Programme (FP7/2007-2013) / ERC grant agreement n$^{\circ}$
[614922]. PAS acknowledges support from the Ram{\'o}n y Cajal
Programme of the Spanish Ministerio de Economía, Industria y
Competitividad.

redpajama_set_name: RedPajamaArXiv


text:
Women's Soccer: Potent offense proves plentiful in win
Casey Delich
Visiting Michigan became another victim of CSUN's women's soccer teams' stingy defense, losing 1-0 at Matador Field Thursday night.
Matador freshman Cori Deason (second from left) celebrates her first goal as a Matador while teammate Brittanie Sakajian (right) makes her way over to join in. Photo credit: Danielle Hale/ Daily Sundial
Meeting for the first time, Michigan(4-1) looked overmatched from the start, and became the first Big-10 school CSUN has ever beaten.
The match was hotly contested throughout, with CSUN(3-1-1) showcasing its offensive pressure throughout the first half, with Michigan able to withstand the onslaught to end the first half 0-0. Though during the second half, Michigan was able to finally put some pressure on CSUN's vaunted defense, and turned the match into a physical one, that almost resulted in fights.
Both teams committed three fouls in the first half, but the second half saw the teams combine for 18, including the games only yellow card against Michigan.
Freshmen forward Lyndsey Preston attributed it to the intensity that the team has shown.
"We don't want to lose at home, it shows on the team and when we are on the field."
CSUN was able to force pressure on Michigan's defense and their goalie, Haley Kopmeyer, throughout the first half, but were never able to put the ball in the net. A jumping save by Kopmeyer on a header kept the game scoreless.
Preston was part of the attack on Kopmeyer that was unable to convert the pressure into a goal.
"We needed to find opportunities, and we came out in the second half more aggressive after taking a break during halftime," Preston said.
Michigan was unable to put a shot on goal throughout the first half until the 44th minute, showcasing CSUN's lockdown defense.
"In the first half we were in good control of the game," said head coach Keith West.
After multiple missed attempts in the first half, CSUN was able to break through in the second. Redshirt freshman midfielder Cori Deason took a left cross from senior defender Stephanie Norton, and was able to thread the ball into the lower right side of the goal past a diving Kopmeyer.
It was Deason's first goal of her career at CSUN.
"I still am shaking it just feels amazing, and I'm just glad I could make my team proud," Deason said. "I was following Coach West's advice to stay wide and just tried to get the cross kick, and I was able to get it thru two defenders and score."
Michigan woke up in the second half, and got senior goalie Cynthia Jacobo involved in the game, making some incredible saves to preserve the shutout. In the 68th minute, Jacobo made a sliding save on a one-on-one opportunity, the closest Michigan would get to scoring all night.
"I saw she went straight through the line, and knew I had to make a play on her," said Jacobo. "We were able to hold strong, we all wanted the win and shutout."
Jacobo finished the game with three saves, earning her third shutout of the season, and 19th of her career, 7.5 short of the record. Earning her 25th win puts her five short of CSUN's all-time wins record.
Senior forward Marisa Miller went down with an injury on a play in the 78th minute, and had to be helped off the field by the training staff. The extent of her injury was unknown after the game.
Off to their best start in recent memory, West attributes this team's success to the experience and talent that they have.
"We have good players and when you have good players you have a chance to win every game," said West.
"Working hard in practice and outside of practice as much as we can along with the chemistry has really helped us get these wins," said Jacobo.
Casey Delich, Author


text:
Idaho Juvenile Rules (I.J.R.)
Part I. Scope and Purpose of Rules
1. Scope and purpose of rules.
Part II. Juvenile Corrections Act (J.C.A.) Proceedings
2. Jurisdiction under the J.C.A. (J.C.A.)
3. Issuance of summons/subpoena (J.C.A.)
4. Form of summons (J.C.A.)
5. Service of summons (J.C.A.)
6. Admit/deny hearing - Nature of proceeding - Notice - Explanation of rights - Plea - Setting of evidentiary hearing (J.C.A.)
7. Detention and hearing (J.C.A.)-Detention or protective supervision prior to adjudication.
8. Notice of detention (J.C.A.)
9. Right to counsel (J.C.A.)
10. Change of Venue (J.C.A.)
10a. Transfer of probation for courtesy supervision. (J.C.A.) Repealed July 1, 2019.
10b. Transfer of probation in its entirety. (J.C.A.) Repealed July 1, 2019.
11. Informal adjustment (J.C.A.)
12. Pretrial conference (J.C.A.)
12.1. Mediation in criminal cases.(J.C.A.)
13. Notice of further proceedings (J.C.A.)
14. Order setting pretrial conference, evidentiary hearing, or sentencing hearing (J.C.A.)
15. Evidentiary hearing (J.C.A.)
16. Expanding a Juvenile Corrections Act proceeding to a Child Protective Act proceeding (J.C.A.)
17. Sentencing hearing (J.C.A.)
17a. Correction or Modification of Juvenile Sentence (J.C.A.)
18. Revocation of formal probation order; revocation of informal adjustment; and entry of adjudication order (J.C.A.)
19. Standards for commitment to the Department of Juvenile Corrections (J.C.A.)
20. Release from state custody (J.C.A.)
21. Application of Idaho Criminal Rules (J.C.A.)
22. Proceedings by telephone conference or video teleconference (J.C.A.)
23. Right to bail (J.C.A.)
24. Right of appeal under the J.C.A. (J.C.A.)
25. Enforcement of a court order directed to a juvenile's parent[s], legal guardian, custodian, or other person made a party to a Juvenile Corrections Act proceeding (J.C.A.)
26. Discretionary Waiver of Jurisdiction Under the Juvenile Corrections Act.
27. Transfer to Juvenile Court.
28. Expungement.
Part III. Child Protective Act Proceedings (C.P.A.)
29. Application of other rules (C.P.A.)
30. [Reserved].
31. Emergency (pretrial) removal of a child and/or offender (C.P.A.)
32. Notice of emergency removal (C.P.A.)
33. Summons (C.P.A.)
34. Order of Removal (C.P.A.)
35. Guardian Ad Litem Programs (C.P.A.)
36. Guardian Ad Litem (C.P.A.)
37. Right to counsel (C.P.A.)
38. Stipulations (C.P.A.)
39. Shelter care hearing (C.P.A.)
40. Notice of further proceedings Including Parents, Foster Parents and Others (C.P.A.)
41. Adjudicatory hearing (C.P.A.)
42. Extended home visits (C.P.A.)
43. Judicial Review of Placement (C.P.A.)
44. Case Plan Hearing/Permanency Hearing - Aggravated circumstances (C.P.A.)
45. Review hearings (C.P.A.)
46. Annual permanency hearings.
47. Modification or revocation of disposition or case plan (C.P.A.)
48. Termination of parent-child relationship (C.P.A.)
49. Right of Appeal (C.P.A.)
50. Transfer of Venue (C.P.A.)
Part IV. Rules Having Joint Application
51. Application of Idaho Rules of Evidence (C.P.A.) (J.C.A.)
52. Closed hearings (C.P.A.) (J.C.A.)
53. Release of information (C.P.A.) (J.C.A.)
54. Proceedings under I.C. § 20-511A.
55. Review of Voluntary Out-of-Home Placements
56. Declaration
57. [Reserved.]
Part V. Miscellaneous
58. ICWA (C.P.A.)
60. Title and effective date.


text:
// Copyright (c) 2016 Klemens D. Morgenstern
//
// Distributed under the Boost Software License, Version 1.0. (See accompanying
// file LICENSE_1_0.txt or copy at http://www.boost.org/LICENSE_1_0.txt)

#ifndef BOOST_PROCESS_POSIX_IO_SERVICE_REF_HPP_
#define BOOST_PROCESS_POSIX_IO_SERVICE_REF_HPP_

#include <boost/process/detail/posix/handler.hpp>
#include <boost/process/detail/posix/async_handler.hpp>
#include <boost/asio/io_service.hpp>
#include <boost/asio/signal_set.hpp>

#include <boost/fusion/algorithm/iteration/for_each.hpp>
#include <boost/fusion/algorithm/transformation/filter_if.hpp>
#include <boost/fusion/algorithm/transformation/transform.hpp>
#include <boost/fusion/view/transform_view.hpp>
#include <boost/fusion/container/vector/convert.hpp>

#include <functional>
#include <type_traits>
#include <memory>
#include <vector>
#include <sys/wait.h>

namespace boost { namespace process { namespace detail { namespace posix {

template<typename Executor>
struct on_exit_handler_transformer
{
    Executor & exec;
    on_exit_handler_transformer(Executor & exec) : exec(exec) {}
    template<typename Sig>
    struct result;

    template<typename T>
    struct result<on_exit_handler_transformer<Executor>(T&)>
    {
        typedef typename T::on_exit_handler_t type;
    };

    template<typename T>
    auto operator()(T& t) const -> typename T::on_exit_handler_t
    {
        return t.on_exit_handler(exec);
    }
};

template<typename Executor>
struct async_handler_collector
{
    Executor & exec;
    std::vector<std::function<void(int, const std::error_code & ec)>> &handlers;

    async_handler_collector(Executor & exec,
            std::vector<std::function<void(int, const std::error_code & ec)>> &handlers)
                : exec(exec), handlers(handlers) {}

    template<typename T>
    void operator()(T & t) const
    {
        handlers.push_back(t.on_exit_handler(exec));
    };
};

//Also set's up waiting for the exit, so it can close async stuff.
struct io_service_ref : handler_base_ext
{
    io_service_ref(boost::asio::io_service & ios) : ios(ios)
    {

    }
    boost::asio::io_service &get() {return ios;};

    boost::asio::signal_set *signal_p = nullptr;

    template <class Executor>
    void on_setup(Executor& exec)
    {
        //must be on the heap so I can move it into the lambda.
        auto asyncs = boost::fusion::filter_if<
                        is_async_handler<
                        typename std::remove_reference< boost::mpl::_ > ::type
                        >>(exec.seq);

        //ok, check if there are actually any.
        if (boost::fusion::empty(asyncs))
            return;

        std::vector<std::function<void(int, const std::error_code & ec)>> funcs;
        funcs.reserve(boost::fusion::size(asyncs));
        boost::fusion::for_each(asyncs, async_handler_collector<Executor>(exec, funcs));

        wait_handler wh(std::move(funcs), ios, exec.exit_status);

        signal_p = wh.signal_.get();
        signal_p->async_wait(std::move(wh));

    }

    template <class Executor>
    void on_error(Executor & exec, const std::error_code & ec) const
    {
        if (signal_p != nullptr)
        {
            boost::system::error_code ec;
            signal_p->cancel(ec);
        }
    }

    struct wait_handler
    {
        std::shared_ptr<boost::asio::signal_set> signal_;
        std::vector<std::function<void(int, const std::error_code & ec)>> funcs;
        std::shared_ptr<std::atomic<int>> exit_status;

        wait_handler(const wait_handler & ) = default;
        wait_handler(wait_handler && )      = default;
        wait_handler(
                std::vector<std::function<void(int, const std::error_code & ec)>> && funcs,
                boost::asio::io_service & ios,
                const std::shared_ptr<std::atomic<int>> &exit_status)
            : signal_(new boost::asio::signal_set(ios, SIGCHLD)),
              funcs(std::move(funcs)),
              exit_status(exit_status)
        {

        }
        void operator()(const boost::system::error_code & ec_in, int /*signal*/)
        {
            if (ec_in.value() == boost::asio::error::operation_aborted)
                return;

            int status;
            ::wait(&status);

            std::error_code ec(ec_in.value(), std::system_category());
            int val = WEXITSTATUS(status);
            exit_status->store(status);

            for (auto & func : funcs)
                func(val, ec);
        }

    };
private:
    boost::asio::io_service &ios;
};

}}}}

#endif /* BOOST_PROCESS_WINDOWS_IO_SERVICE_REF_HPP_ */

redpajama_set_name: RedPajamaGithub