USB connector was developed in the 1990s, which is abbreviation for Universal Serial Bus. It was designed to facilitate the connections between peripheral devices and computers. And owing to its compatibility with many paltforms and operating systems, years later, it was widely used in many fields of its low cost and high efficiency.
Today, most computers are built with many USB ports. Also, USB connector is a good choice for homes or office peripherals, such as cameras, modems and printers. This post we want to analysis the classification of USB connector.
The standard of USB connector was developed and maintained by an industry body, which was called the USB Implement Forum (USB-IF). And in the original design, USB connector can divided into two types: Type A and Type B. Later, for the demands on manufacturers and performance, it has expanded scope of ese. And then Type C （Usb type C you need to know） was appeared.
This picture we can comprehend the classification of USB connectors in a flagrant contrast.
- USB Type A connectors (Standard-A connectors) are flat and rectangular in shape. It can be supported in each USB version, both in USB 3.0, USB 2.0, and USB 1.1. And Type A was the “original” USB connector. Also, it was the most recognizable and commonly used connector.
- USB Type B connectors are at the other end of a typical USB cable that plugs into a peripheral device, such as a smartphone, a printer or a hard drive.
- USB Type C connectors, the newest USB connector on the market, have designed to be plugged into many USB-C device. And Type C cable is capable of carrying USB 3.1, USB 3.0, USB 2.0 and USB 1.1 signals.
Due to its compatibility with many fields, USB connector are widely used in peripheral devices and computers. And you can scan other pages to see more about USB connectors at elecbee. Elecbee.com is a electronic conponents store whom sell RF coaxial connector, USB connectors and Antennas. Free for all order over $99.00.
Welcome to contact us if you are interested in USB connectors. We provide personalized customization or wholesale.


Queenslander Matthew Guyatt is proving he is more than just an opening-round bolter, bursting out of the blocks on day two to open up a big lead in the Australian Masters.
Guyatt began the day two shots ahead of three players tied for second, including tournament headliners Adam Scott and Ian Poulter, but that gap has ballooned to five shots on the back of a lightning first nine holes.
Guyatt has jumped from seven-under to 11-under thanks to four birdies, two coming back-to-back on the par 4 3rd and 4th holes.
New Zealander Michael Hendry has picked up one shot on his overnight score to move to outright second at six-under after five holes this morning, while a bogey on the par 3 15th (his 6th hole today) has meant Poulter is still at five-under.
Top-ranked Australian Scott will begin his second round at 12.10pm this afternoon at five-under, likely knowing he will need something special to keep pace with Guyatt.
There is a further five players behind Poulter and Scott tied for fifth at four-under.
Former Masters champion Stuart Appleby has endured a difficult morning so far, bogeying his third and sixth holes to slip back to one-over after starting his round at one-under.


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“Mark your calendars for Sunday afternoon, June 25 at 3:00 pm, as Mazzoni Center is coordinating Philadelphia’s Interfaith Pride Service, to be held at Arch Street Presbyterian Church (1724 Arch Street)
Mazzoni Center has been working with a diverse group of interfaith clergy to create an engaging and affirming service aimed at fostering a spirit of love, recognition, understanding, unity, and support among all participants, including readings, music, and creative ritual.
Organizations partnering to support the Interfaith Pride Service include Attic Youth Center, Bebashi, COLOURS, galaei, Independence Business Alliance: Greater Philadelphia’s LGBTQ+ Chamber of Commerce, Jewish Federation of Greater Philadelphia, Philadelphia Black Pride, Philadelphia FIGHT Community Health Centers, Tribe 12, and William Way LGBT Community Center. It is hoped that this will be the first of what will become a treasured annual event”
Tribe 12 connects people in their 20s/30s to Jewish life and community in Philadelphia today so they will choose to stay connected tomorrow. We welcome people who identify as Jewish, whose partner is Jewish, or who are exploring Judaism. Tribe 12 seeks to include all individuals regardless of gender or identity expression, religious history and practice, health and disability whether visible or invisible, and financial circumstances. For questions, to request accommodations, or just to say hi, reach out to firstname.lastname@example.org.

domain: news


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market review : europe & us
European shares saw red while US shares ended marginally higher led by tech stocks after surviving another disappointing data on consumer sentiment. German DAX index fell 39.89 points or 0.64% at 6,209.76 and FTSE 100 finished 31.69 points lower or down 0.57% at 5,508.45. Tech stocks led US shares on Friday as Nasdaq Composite gained 0.54% or 12.36 points to 2,315.61, while Dow Jones Industrial Average posted a marginal gains of 13.02 points or 0.12% to end at 10,607.85. S&P 500 index inched 0.08% higher to 1,125.59.
Irish Finance Ministry denied rumors that the country was in need for International Monetary Funds’s assistance to help its ailing banking sector. The rumor sent the Irish credit default swap to hit 425 basis points, a record high. Ten-year bond yield also rose to around 6.5%, as well as yield premium over German Bunds to 410 basis points, also a record high. EURUSD was shot down from mid-1.31s to the lower 1.30s after the news before it stabilized at 1.3040s at the end of the day. Despite the denial, the news – which was based on Barclays’ research note – brought back the concerns over the fiscal health over European countries.
Consumer Sentiment took a blow in September as the index from The Thomson Reuters/University of Michigan reported it falling to 66.6 from 68.9 in August. Current economic conditions was nearly unchanged in September as it stood at 78.4 against the August reading of 78.3 Consumer expectations index declined to 59.1 in September from 62.9 in August. All three indexes were below the consensus : the sentiment index was initially expected at 70.00, while current economic conditions index and consumer expectations index were forecast at 79.0 and 64.2, respectively.
Another data due on Friday was Consumer Price Index (NYSEARCA:CPI) which showed a month-on-month gains of 0.3% in August. Its core measure, which omitted the prices of food and energy was unchanged. Market consensus initially expected the headline CPI to rise 0.2% while the core index to also gain 0.1%. Year-on-year, headline index was up 1.1% and the core index was up 0.9% in August. Timid readings would mean that the Federal Reserve - which is going to meet again next week – is most likely to keep interest rates on hold at 0.25%.
European data on Friday featured German Producer Price Index which was flat in August on month-on-month terms, slower than July’s 0.5% gains. Compared to a year earlier, PPI also slowed to 3.2% in August from 3.7% gains in July. Construction output in Euro-Zone fell 3.1% in July after rising 1.8% in June on month-on-month basis, but suffered from a worse fall of 7.5% in year-on-year terms after gaining 1.9% in June.
Post-earnings report, several houses revised their expectations on Oracle Corporation. Piper Jaffray raised Oracle’s target to $31 from $30 and maintaining its OVERWEIGHT rating; Citigroup also raised the price target to $30 from $28; FBR Capital kept Oracle at OUTPERFORM while raising its target to $32 from $30; RBC Capital also hold its rating at OUTPERFORM with target raised to $32 from $28; and JMP Securities set price target at $33 and raised its rating to OUTPERFORM from MARKET PERFORM. Oracle leaped 8.36% to settle at $27.48 on Friday.
Johnson & Johnson is to acquire Crucell for $2.3 billion. The bid for the vaccine maker worth 24.75 euros per share, which means a premium over 50%. Opening up the door to the vaccine market will put J&J in competition with the drug giant GlaxoSmithKline Plc. J&J rose 0.46% to $61.57 on Friday.
Citigroup Inc. sold its student loan business to Discover Financial Services and SLM Corp. (a.k.a. Sallie Mae). Discover will pay $600 million for the stake, including $4.2 billion worth of loans, and Sallie Mae will acquire $28 billion of assets, including 1.3 million new customer. Citigroup will bear a loss worth $500 million, which will be included in the Q3 report. Citigroup ended at $3.95 or down 0.5%.
Microsoft’s price target was lowered to $30 fom $35 by Oppenheimer, but retained its rating at OUTPERFORM. The house pointed at ‘increasing headwind’ in both Windows PC & Office businesses as the factor behind the revision. Meanwhile, FBR Capital also kept Microsoft at OUTPERFORM as well as its price target at $32. However, slowing PC demand led to revisions of earnings estimates: 3Q to $0.54 from $0.56, and for June 2011 fiscal year from $2.38 to $2.31.
Volkswagen AG’s Czech unit Skoda Auto AS announced its plan to introduce a new model soon. The news pushed the price of its preferred shares up 2.6% to €91.21.
Barclays Plc shed 3.2% on Friday, settling at 304.65 pence after UBS downgraded its earnings estimates by 8% for 2010, 13% for 2011, and 20% for 2012.
McDonald’s was rated at HOLD by Jefferies, with target set at $75.
next week preview
Key US data for next week will be dominated by housing data: NAHB Housing Market Index for September, expected to rise from 13 to 14; Building Permits which are seen to inch higher to 560k in August from 559k in July; August Housing Starts, with the consensus of 550k against prior 546k, slowing down from 1.7% gains in July to 0.7% in August; and House Price Index which is expected to fall 0.1% in July after a drop of 0.3% in June. More housing data due are Existing Home Sales, expected to show a bounce as it is seen to rise 7.1% in August to 4.1 million after a plunge of 27.2% in July and finally, New Home Sales, which is expected to show gains of 6.9% in August after slumping 12.4% in July.
Other than housing data, Federal Reserve’s FOMC meeting will be the focus even that the rates are likely to stay on hold. US leading indicators for August will be released in Thursday, it is expected to show a 0.1% gains, the same pace as July’s; while Durable Goods Orders are expected to show a rise of 1.4% after it gained 0.4% in July. Excluding transportation items, orders are seen rising 1% in August after it dropped 3.7% in July.
Data from Europe will be German Manufacturing PMI for September, seen at 57.6 against 58.2 in August; the PMI for Services, seen unchanged at 57.2; while Euro-Zone PMI for Manufacturing is seen at 54.5, down from 55.1 in August; For Services, the PMI is seen slightly lower at 55.5 in September against 55.9 in August; and finally the Composite PMI Index is expected at 55.7 in September compared to August’s 56.2. Another gauge of output for Euro-Zone, industrial new orders are seen slowing to 16.2% (y/y) in July from 22.8% gains in June; month-on-month, the orders are seen to have fallen 1.4% in July after it posted gains of 2.5% in June.
Consumer confidence data will also due in Europe. The first would be from Euro-Zone and it is expected to improve to -10 from -11 in September, while the second will be the German IFO index. IFO’s business climate index is seen down to 106.4 from 106.7 in September; while the current assessment index is seen improving to 108.7 from 108.2; however, the expectations index is seen falling to 104.0 from 105.2.
A day after the Fed delivers its decision on rates, the Bank of England will release its latest MPC minutes on Wednesday. The minutes will show how the Bank assessed the economy during its latest meeting and how the balance of votes was. The last time, eight members voted for no changes in rates, while Andrew Sentance voted for a rise in rate of 25 basis points.
Disclosure: No Positions

domain: finance


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Conversations about statehood for Puerto Rico can reveal some surprising misconceptions. For example, Rick Santorum demonstrated that he thought states had to have English as their official language (the U.S. doesn’t have an official language, and there is no such requirement). There have been discussions on our Facebook page about whether the current states would have to ratify Puerto Rico’s admission (nope). Another common belief is that the U.S. can only admit states in pairs.
In December of 1787, three new states were admitted: Delaware, Pennsylvania, and New Jersey. Georgia and Connecticut were admitted within a week of each other the following month, and three more states were admitted in February, April, and May, with two more in June and one in July. Clearly, early states weren’t admitted in pairs back in the early days of our nation.
So where did we get the idea that states could only come into the Union two by two, like animals on Noah’s Ark?
It started in 1812, when the states were evenly divided between those that had given up or were planning to give up slavery, and those that were committed to keeping slavery. States admitted over the next few years ended up maintaining that balance, and when Missouri’s admission was discussed in 1820, Maine was brought in ahead of Missouri to keep things even.
This is a strange idea for us nowadays. Americans have agreed that slavery is a terrible thing. We still have issues on which we’re divided — gun control, abortion, climate change, and more — but we don’t try to solve those differences by keeping an equal number of our legislators on each side. That’s how it was done in the 1800s, though.
States weren’t admitted together, but people were keeping track and made an effort to keep things fairly even. When California joined in 1850, at which point states with and without slavery were even, it was agreed that California would send one Senator who favored slavery and one who did not.
After the Civil War, slavery became a moot point. Still, it had become a habit. President Benjamin Harrison brought in six new states, in three neatly matched pairs of Republican and Democratic states. Taft brought in New Mexico and Arizona in 1912 and Eisenhower welcomed Alaska and Hawaii in 1959. In between, there were single state admissions, but the relatively large number of paired states stayed in the public imagination.
Many Americans now believe that there is a law requiring a Republican state and a Democratic state to join together to maintain the balance — apparently, we’ve forgotten that the required balance was originally between slave and free states.
This is not true, any more than a state is required to have English as an official language. There have been several sister states suggested for Puerto Rico, including the District of Columbia, but there is no such requirement. Puerto Rico can join on her own.
This post was originally written in English and may be being auto-translated by Google.

domain: history


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If you’ve got airline points or miles saved up, you could hang on to them in the hopes that you might be able to redeem them for a flight at some point—but if you don’t see yourself boarding a plane any time soon, you might as well see if there’s some other way to redeem those miles.
Why? Because, as we’ve noted previously, there’s no guarantee that the value of your points or miles will stay constant over time. Airlines continually update their rewards programs, and “earning and burning” is one of the best ways to maximize those rewards.
Plus, you might be able to turn your airline rewards into something you can use right away. As The Points Guy reminds us, it’s still possible to use travel rewards on non-travel rewards—though some travel loyalty programs have temporarily suspended some of their redemption perks, specifically limiting gift card redemptions. (The Points Guy also reminds us that some airlines might go bankrupt as a result of the pandemic, in case you wanted another incentive to use up your rewards while you still have them.)
Here’s what I found when I did a quick survey of the major airlines. I’m not including flight, hotel, or vacation package redemption options, which are still widely available; instead, I’m sharing ways to redeem your miles without leaving your home.
Delta Air Lines
JetBlue TrueBlue points can be redeemed for charitable donations.
Although Southwest’s More Rewards page is still live, when you try to redeem Southwest Rapid Rewards for a non-travel reward, you get the following message:
Due to circumstances resulting from COVID-19, we have temporarily paused the ability to redeem points in More Rewards. We are sorry for the inconvenience and hope to resume normal operations soon. Thank you for your patience and grace during this time.
If you have a non-airline-specific travel credit card like the Chase Sapphire Preferred, you should have even more reward redemption options—and yes, I know that your travel and airline rewards decrease in value if you redeem them for stuff that isn’t travel-related. You can decide if it’s worth using up your rewards now, even at a slightly lower value, or saving them for the indefinite future.
You might also want to consider switching your spending to a cash-back rewards card—because if you’re going to be staying home for a while, you might as well take advantage of a little extra cash.

domain: travel


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May 17, 2023
Lisa: We Ride Upon Sticks by Quan Barry (book)
Andrea G.: Big FIght in Little Chinatown (film)
Andrea W.: Love in Color: Mythical Tales from Around the World, Retold by Bolu Babalola (book)
Louise Burns: Baywatch (TV); The Dark Crystal: Age of Resistance (Netflix)
Pop This! is a podcast featuring three women talking about pop culture.
Lisa Christiansen is a broadcaster, journalist and longtime metal head. Andrea Warner is a music critic, author and former horoscopes columnist. Andrea Gin is a producer and an avid figure skating fan.
Press play and come hang out with your new best friends.
Pop This! podcast is produced by Andrea Gin.

domain: artistic


Motorola has recently launched Moto G Turbo Edition in India as the successor of Motorola Moto G3. The phone looks similar to the Moto G3 in terms of design as well as Specification with a little upgrade. Talking about the technical specification of Moto G Turbo, it has the 5inch HD display with 1280 x 720 Pixels protected by the Corning Gorilla Glass 3. The Moto G Turbo is powered by the enhanced 1.5 GHz Snapdragon 615 Octa-Core processor aided by the 2GB RAM. The internal storage of the device is 16GB and also has expandable Micro SD Card support up to 32GB. The Moto G Turbo runs on the Android Lollipop 5 with Stock UI and there is also a high chance for Moto G Turbo to get the Android M update. One of the special features of the Motorola G Turbo is its IP67 Water Resistant and Turbo Charging feature. The phone is packed with 2470 mAh battery which is not user removable. It has the same 13MP rear camera with LED Flash and 5MP front camera as found in Moto G(3rd gen). The phone is priced at Rupees 14,999 in India exclusively via Flipkart. Here are the Motorola Moto G Turbo Pros and Cons, FAQ and user queries answered.
Moto G Turbo Edition FAQ & User queries answered
Q: What are the box content of the phone?
A: The phone itself, Turbo charger ( Motorola hs provided the turbo charger in the box itself this time), Normal quality Earphone, Warranty card and user manual. The USB cable cannot be detached from the charger adaptor so you need to buy separate USB cable to sync the data to the system.
Q: Does the Moto G Turbo Edition has the Corning Gorilla Glass 3 protection?
A: Yes, the phone display is protected by the Corning Gorilla Glass 3 on the top to protect the phone from cracks and scratches.
Q: What is the free internal storage available on the device?
A: Around 10.49 GB is user available for installing Apps and Games out of 16GB onboard storage.
Q: Does the Moto G Turbo has the LED Notification light?
A: No, the phone does not have the LED Notification light. But the Active display feature acts as the notification option.
Q: What is the difference between Moto G Turbo Edition Vs Moto G(3rd Gen).
A: There is no difference between Moto G Turbo and Moto G 3rd Generation in terms of design. On Specification side, Moto G Turbo has the 1.5 GHz Snapdragon 615 processor and Turbo Charging feature. Whereas the Moto G(3rd gen) has 1.4GHz Snapdragon 410 processor and does not have the Turbo Charging feature.
Q: What is the free RAM available after the first boot?
A: Out of 2GB RAM, around 1.2GB is free after the first boot.
Also Read: Top 40 inch LED TV available in India
Q: Can we move Apps and Games to SD Card in Turbo Edition?
A: Yes, Some part data of the Apps and Games can be moved to the external Micro SD Card.
Q: How is the gaming performance of Moto G Turbo Edition? Is there any heating issue?
A: The phone can able to handle some of the HD games like Dead trigger 2, Hitman Snipper, Asphalt 8. There is no serious heating issue with the phone.
Q: Does the phone has the OTG Support?
A: yes, the phone has the OTG support for connecting Pendrives, mouse, keyboard and gaming controllers.
Q: Does the phone has the Micro SD Card support?
A: Yes, the Moto g Turbo has the expandable Micro SD Card support which supports up to 32GB Card.
Q: What is the Turbo charging feature on the phone?
A: It is the Fast charging which would charge your 2470 mAh battery in just 1 hour 30 minutes.
Q: How is the call quality of the device?
A: The call quality is clear and loud and there are no issues with the network.
Q: Does the phone have the video calling feature?
A: There is no inbuilt video calling feature, but it can be supported using 3rd party Apps.
Q: What is the SAR Value of Moto G Turbo Edition?
A: The SAR value of the phone is 0.905 W/Kg at the head and 1.069 W/Kg at the body.
Q: How is the camera quality of the phone?
A: The camera quality of 13MP rear and 5MP front is good enough. The rear camera can record HD 1080p videos and it also has slow motion recording option.
Q: Does the Moto G Turbo Edition has the Water resistance feature?
A: Yes, the phone has the IP67 certification and yes it is the water resistant and dust resistance smartphone.
Q: What are the color option available and how to buy the phone?
A: The Moto G Turbo comes in White & Black color variant. The phone is priced at Rupees 14,999 in India and exclusively available via Flipkart. You can use the link below to buy the Smartphone.
|Moto G Turbo Black||[su_button url=”http://fkrt.it/geHu3uuuuN” target=”blank” background=”#0db735″ size=”4″ icon_color=”#000000″ rel=”nofollow”]Buy Now[/su_button]|
|Moto G Turbo White||
Motorola Moto G Turbo Edition Pros and Cons
Here are the advantage and disadvantage (Pros & Cons) of Moto G Turbo.
Battery drains little fast
Normal quality Earphones
So these are the some of the frequent user queries, pros and cons of Moto G turbo. The phone is one of the best options for the 15,000 Rupees price segment. This would give tight competition to Lenovo VIBE P1, Asus Zenfone 2 (2GB RAM). If you have any further queries about the phone please leave them in the comment section below. For more FAQ posts and device information, follow us on Facebook, Twitter, and Pinterest.


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I like Barry Adam because when I ask him if being gay is the most important thing about his identity, he replies, “It is important. I’m not one of those people who says, ‘It doesn’t matter,’ because we are not all the same.”
Adam is an internationally acclaimed sociology professor at the University of Windsor and the senior scientist and director of prevention research at the Ontario HIV Treatment Network. He has studied, taught and written about queer identity, global gay and lesbian politics, and HIV for more than three decades, and he will close Concordia University’s 2011/12 HIV/AIDS lecture series on March 15 with a lecture called “Neoliberalism, Masculinity, and HIV Risk.”
The notes for Concordia’s landmark series read, “While Dr Adam’s work remains grounded in grassroots knowledge and experience, he argues that intellectual traditions such as feminism, postcolonial and queer theory remain crucial in disrupting ideas created by the neoliberal environment in which HIV was discovered. His lecture will look at how the face of the pandemic has been influenced by an environment in which the populations most affected by HIV were already subordinated. Only when we recognize this, he argues, can we begin to develop an effective prevention and education campaign and health care programs for those living with HIV.”
In other words, Adam says, neoliberalism has a lot to answer for.
“The reason gay men have unprotected sex is largely psychological, ranging from personality traits to depression, and what I’m trying to do is rethink all of this research and literature in the larger environment gay men are in to explain these factors,” he explains. “The neoliberalism part has to do with masculinity in our society and how we conceive of infectiousness.”
But wait, there’s more. “One of the strange things about neoliberalism is it is a morality, about how neoliberals do good in the world. They do not see themselves as destructive or responsible for bad things. So I want to draw attention to their unintended consequences.”
Adam, author of The Rise of a Gay and Lesbian Movement (1995) and Experiencing HIV (1996), is also editor of The Global Emergence of Gay and Lesbian Politics (1999). He has long voiced strong opinions about the politics and social issues surrounding HIV and AIDS but these days seems reluctant to get drawn into the crossfire over controversial posters seen at demos in Toronto, Ottawa and Montreal ahead of the Feb 8 Supreme Court of Canada hearing of two landmark cases about HIV, sex and criminal law.
One poster, by artist Mikiki and Scott Donald, from AIDS Action Now’s 2011 “Poster/Virus” series, reads, “I Party, I Bareback, I’m Positive, I’m Responsible.” It ignited a firestorm in Montreal’s HIV/AIDS communities.
“I grew up in the days of gay liberation, and I am of that generation where many of my friends and lovers died of AIDS,” Adam says. “So the subject of HIV and AIDS strikes very close to home. I know one of the originators [of that poster], and he is just raising questions about serosorting. It is possible to serosort and he has a point. I also think that he is just trying to rile people up. But if this is regarded as a free-for-all, you can see why people would be upset and rightfully so.”
Adam will field questions during a lengthy Q&A session following his lecture at Concordia.

domain: sociology


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When a relationship breaks down, it’s common and understandable to feel alone and worried. How you choose to represent yourself in a divorce will affect the rest of your life. You’ll want someone to always have your best interests at heart and fight your corner relentlessly. That’s where our team of Divorce Solicitors come in.
If you’re going through a divorce, there’s a lot to think about. You’ll need to decide what happens to your money, property and children if you have any. From property to pensions, our Specialist Team of Divorce Solicitors in Manchester are here to help.
With 170 years of experience, you’re in safe hands with Simpson Millar. No matter how complex or straightforward, there’s not much we haven’t come across. We know divorce can get messy. That’s why we always try to keep things as amicable as possible while still offering you the best legal protection. We advise compassionately and work in your best interests.
We offer sound legal advice and our Divorce Solicitors in Manchester offer a Fixed Fee Divorce. This means you know exactly how much your divorce is going to cost, with no nasty surprises. If you’re interested, read on to find out more about us and the services we offer.
Divorce Disputes in Manchester
Whether you’ve been married for a couple of years or decades, we’re here to help. Our Manchester Solicitors for Divorce specialise in all sorts of disputes and can offer expert advice on:
- The Grounds for Divorce
- Your Divorce Petition
- Overseas Divorce
- Defending a Divorce
- Cross Petitions
- Civil Partnership Dissolution Hearings
- Judicial Separations
Are you worried about the implications of divorce on your finances? If so, we’ll advise you on the best Financial Settlement to protect you and your future.
Why Choose Us as Your Divorce Solicitors in Manchester?
Getting a divorce can be complicated, but it doesn’t have to be. At Simpson Millar, we aim to make the process as simple and quick as possible. Whether you and your ex agree or not, we’ll put you first and strive to settle things amicably. If we can avoid going to Court, we will.
Here are just a few reasons why you should trust us to represent you if you’re looking for a Divorce Solicitor in Manchester:
- We offer a Fixed Price Divorce in our Manchester office, so you can be certain of what you’ll pay before you commit. We’ll always let you know the cost beforehand, so you can budget properly
- Our Divorce Solicitors in Manchester keep your best interests at heart. We promise to always fight your corner and get you the best deal we can for. We’re not stuffy. Our people are friendly, honest and trustworthy
- We don’t believe in difficult-to-understand legal jargon. We’ll speak to you in plain English and make sure you understand the divorce process from start to finish. Our friendly advisors are always happy to answer your questions
- We believe communication between parties is key, so we’ll work diligently with you to help settle matters without going to Court. We’ll avoid a Court battle unless it’s not possible, saving you time, money and stress
- We’ll make sure your interests are protected financially, both now and in the future. Our people are experts in Financial Settlements and will work to get you the best deal possible
- If dealing with your husband or wife is daunting, we’ll negotiate the settlement for you. If you don’t want to deal with them at all, you won’t have to
- We hold the Law Society’s Family Law Accreditation so you can be confident your family matters are being looked after by leading industry professionals
- We’re rated as ‘Excellent’ on Trustpilot. Why not take a look at how we’ve supported other people like you?
Contact Our Divorce Lawyers in Manchester
If you’ve had a relationship breakdown, get in touch with one of our Divorce Solicitors in Manchester today. Once we understand your situation, we’ll offer some initial advice. If you then choose us to represent you, we’ll do everything we can to get you what you deserve.
Contact Our Specialist Divorce Solicitors in Manchester Today
Tel: 0161 516 1890
Fax: 0345 357 9399
Alternatively, you can request a callback and we'll give you a call.
How to Find Us
Our Manchester office is on Talbot Road, close to the junction with Warwick Road. It’s near Old Trafford cricket ground and a short drive from the M602/A57(M) motorways. It has limited on-street parking close by.
The Old Trafford stop on the Manchester Metrolink tram network is less than a 5-minute walk away and is served by regular trams between Altrincham and Manchester city centre. You can find us at:
100 Talbot Road
For initial legal advice call our Family Law and Divorce Solicitors
We're happy to help
Monday to Friday 8:30am-7:00pm
0808 239 3465
We're happy to call you
Simply click below to arrange a call
Simpson Millar Solicitors are a national law firm with over 500 staff and offices in Billingham, Bristol, Cardiff, Catterick, Lancaster, Leeds, Liverpool, London and Manchester.

domain: law


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Activate Transit Windsor Essex (ATWE) | Windsor, Ontario
Jessica is an entrepreneur and community advocate in Windsor. Most recently, she and her partner launched a small urban flower farm focusing on regenerative agriculture practices. She is a member of the Windsor Bicycling Committee and oversees food services at the Welcome Centre Shelter for Women and Families. In 2020, she successfully advocated to restore transit after Windsor was the only city in Canada to suspend service. She is currently working on developing a citizen-led and grassroots transit advocacy organization in Windsor Essex.
About the Project
Activate Transit Windsor Essex (ATWE) is a grassroots organization advocating for the use and advancement of an interconnected public transit system in Windsor Essex. By organizing meetings, focus groups, and online methods of citizen participation, we will create democratic space for citizen-led conversation about the future of public transit and mobility in the region. By creating an engaging web presence, organizing social media campaigns, and publishing responses or propositions for policy, we will create a medium for amplifying the voices of citizens, especially those who have been systematically disadvantaged and underrepresented in the past.

domain: politics


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The City of Chicago has completed the first round of community presentations for the final three casino bids. Earlier this year in March news broke of the mayor selecting the three sites with the first community meetings beginning early in April, this ruled out the Bally’s and Rivers McCormick Place bids, leaving us with Bally’s Tribune, Hard Rock’s One Central, and Rivers The 78 as the remaining choices. While the meetings were to educate the public and answer any questions, they riled up some controversies among local community groups. Recordings of the presentations can be found here.
Hard Rock One Central Bid
The meeting which took place April 6th revealed a handful of new details on the $1.7 billion proposal which is hoping to kick start the mega-development and utilize the McCormick Place Lakeside Center as its temporary location. With a recently launched website, the presenters stated the project would take around 30 months to build while creating over 6,800 and up to 19,000 jobs from construction to operations. It is worth noting that the project has yet to strike a deal with the use of the Lakeside Center, which has been mentioned by its operators to not be a viable option.
Other information disclosed was that funding wouldn’t be an issue for the roughly 35-story tower and casino, stating that the bid has a strong backing from Hard Rock who has done multiple casinos in the past. It was also emphasized that although it will utilize One Central’s land, it wouldn’t be a part of the development, but because of it One Central would be scaled back by roughly 20 percent. The bid received criticism from the neighbors including from the operator of McCormick Place who expressed that some major conferences will not want to host their events near a casino.
Bally’s Tribune Center Bid
Being the bid that has received the largest redesign since its launch, the meeting which took place April 7th within the building that would be their temporary facility revealed further details on the new concept. With an anticipated three-year construction timeline, the proposal would be a part of planned development 1426 which was approved in 2018 for roughly 8.5 million square feet of space. The updated one million-square-foot casino complex will decrease the plan’s overall size to 6.5 million which was used to argue against many of the traffic concerns. Although most in attendance oppose the proposal, the local alderman says there are large groups who didn’t attend support it.
The updated design is being executed by SCB and will pursue LEED certification, the completed $1.7 billion project would deliver a 37-story hotel tower, roughly 3,000 parking spaces in an underground garage, 2,100 feet of riverwalk and parks, as well as a 70,000-square-foot entertainment venue and 20,000-square-foot exhibition space. Also being considered are a new pedestrian bridge over the river, various green spaces, and a rough redesign of the development layout. Along with the push back there was also some controversy with members of neighborhood committees privately meeting with the developers prior to the presentations.
Rivers The 78 Bid
As one of the most anticipated bids, the meeting took place on April 7th and received plenty of negative feedback from area residents who also expressed disdain towards the greater 78 project. The local alderman reported roughly 80 percent of residents surveyed about the proposal opposed it, this was followed up by protesters outside of the presentation and multiple people yelling to the point of having the microphone shut-off. The meeting did bring out a few new details including the confirmation of the riverboat temporary facility and the construction of the future CTA Red Line 15th Street stop.
Other details included highlighting the creation of 4,000 construction jobs, 3,500 permanent jobs, and roughly 5,000 students that will utilize the nearby Discovery Partners Institute that just received their land transfer. It is also worth noting that The 78 Community Advisory Council held a press conference this past week stating they are against the proposal, with some worrying that if the casino bid isn’t won the $7 billion mega-development could be in jeopardy.
The city will now proceed to analyze the feedback from the various presentations and determine if they are ready to make a choice. While there is no clear winner, it is predicted each proposal will deliver a different level of tax revenue, after six years Hard Rock is predicted to bring in $185 million, Bally’s $195 million, and Rivers $174 million. At the moment there is no formal timeline on when a decision could be made, however you can read the journey of the casino selection here.


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We formulate the on-axis asymptotic scintillations of sinusoidal and hyperbolic Gaussian beams, namely cos and cosh Gaussian beam, under strong turbulence conditions. Our results are displayed in the form of plots of the scintillation index against propagation distance and wavelength at several source and propagation parameters. It is revealed that at small source sizes, cosh Gaussian beams will exhibit the lowest scintillations, but at large source sizes, this will reverse and cos Gaussian beams will attain such characteristics. It is further found that in strong turbulence, longer wavelengths will offer less scintillations, a behavior similar to the one, encountered in weak scintillation conditions.


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Sitting on top of Mandalay Hill, Sutaungpyei Pagoda features a large patio that offers a wonderful views over Mandalay City and the Ayeyarwaddy.
Some cameras say they have a silent shutter, but when you go to use it they turn out to just have a very quiet shutter. I've been pleasantly surprised that the one on the Sony a7iii really is silent. Here's how to set it up.
Here's a selection of sample images I've taken with the Sony 35mm ƒ/1.4 ZA lens, one of Sony's high-end E-mount prime lenses.
The Sony 50mm ƒ/1.4 ZA lens is one of Sony's high-end lenses. On full-frame sensors it offers a normal perspective and is especially good for low-light and selective focus shooting. Here are some sample photos I've taken with it.
Wondering how useful the Fujifilm X-T2's high-ISO settings are that go all the way up to ISO 51200? I shot some images to find out.
A selection of sample images I've shot with the Sigma 105mm f/2.8 EX DG OS HSM macro prime lens.
How useful are the Sony a7r iii's high-ISO settings that go all the way up to ISO 102400? I shot some images to find out.
The Sony a7r iii has a well-earned reputation for boasting an extraordinarily good sensor, and it has an ISO range from 50 up through 102400. I shot some real-world examples through the ISO range to see how the ISO settings compare side by side.
The Fujifilm X-T2 has an ISO range from 100 to 51200. Here's a collection of sample images shot across the full ISO range to give an idea of how to performs in real-world shooting.
Heavy snow shuts down Washington DC, but it also transforms the National Mall, its monuments, and other Washington landmarks like the White House into a winter wonderland.
The rugged, mountainous terrain of northern Laos is beautiful. While well off the beaten track and not really on the road to anywhere else, Luang Namtha and Oudomxai provinces are well worth seeing.
If God and the government had their way, Antigua wouldn't exist. But it's a good thing it does. With charming Spanish colonial architecture, cobblestone streets, and a vibrant cultural life, it's a wonderful place to visit.
Central America is where American school buses go to retire. In the balmy tropical climes of places like Guatemala and Honduras, they're given a new, colorful lease on life.
Inside the Citadel walls was once lavish and opulent, with ornate gardens and intricate pagodas. But the Vietnam War was not kind to the Imperial City. Large parts of it are now nothing more than rubble.
Newark, New Jersey, isn't exactly known as a jewel of the American northeast. But from certain vantage points, it can actually be quite pretty. Glittery, even.
That the Lemaire Channel is nicknamed "Kodak Gap" is a pretty good indication that it's reliably scenic. When the conditions are right, it's spectacular.
Ever fancied a pre-breakfast swim with turtles and manta rays? If you've ever had a hankering to get up close and personal with Australia's extraordinary Great Barrier Reef, there aren't many better ways than a trip to Lady Elliot Island Resort.
Here's a detailed breakdown of how the GoPro HERO5 Session compares with the new HERO (2018), including video and photo capabilities.
Although the GoPro HERO (2018) isn't compatible with the Remo or Smart Remotes, there are still a couple of ways to control the camera remotely out of the box.
Here's a rundown of the relevant modes and settings of the photo mode on the GoPro HERO (2018), including file types, fields of view, and enhanced dynamic range.
On the GoPro HERO6 Black and HERO5 Black, you can choose between two image formats for still photos: JPG and RAW. Here's a quick overview of what the difference is and when to use which.
GoPro's QuickCapture feature is designed as a one-press way to power the camera up and start shooting immediately. There are a few tricks to using it, though.
Here's a detailed side-by-side comparison of the GoPro HERO (2018) and the HERO5 Black.
The new HERO (2018) and the HERO6 Black look the same, but there are lots of differences in features and capabilities. Here’s a detailed breakdown of how they compare.
Here's a rundown of the video resolution, framerates, fields of view, and modes that are available on the GoPro HERO (2018).
Here's how to enable the Publish Services, Catalog, Folders, or Collections panels in the Library module if they're not visible.
By itself, Lightroom can't find duplicate photos. But here are a couple of plugins available that can add that functionality.
Here's how to quickly delete rejected photos in Lightroom to help speed up the culling part of the workflow.
A guide to selecting multiple photos in Lightroom.
Both Lightroom Classic CC and Luminar 2018 now offer processing using AI, or artificial intelligence. Here's a side-by-side comparison of their initial automatic one-click processing options.
Luminar 2018 is designed as a standalone app, but you can also use it alongside Lightroom. Here's how to install and use Luminar as a plugin in Lightroom Classic CC.
The Auto tone function has been given a major overhaul in the latest update to Lightroom Classic CC (7.1) to use Adobe's artificial intelligence network, Sensei, in an effort to improve the effectiveness of Auto tone. Here's how it works in practice.
Lightroom's white balance tools help reduce color casts. They can be used to neutralized any casts or break the rules and create an entirely new look.

domain: hobby


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A third arrest was made by Dover Police in connection to the murder of Michael Gklotsos, the late owner of Hollywood Diner.
Dover Police arrested a third suspect Tuesday for the robbery and home invasion that precipitated the murder of Michael Gklotsos, the late Hollywood Diner owner killed Sept. 17.
Dover Police arrested Tiffany Ferraro, 16, of Fairless Hills, Pa., and charged her with robbery in the first degree, conspiracy in the second degree, wearing a disguise during the commission of a felony and home invasion, for her involvement in the break-in of Gklotsos' home, Lt. McKeown said.
Ferraro's apprehension followed the arrests of Joshua Lemonick, 20, of Newtown, Pa. and Angeline Terek, 23, of Bristol Township, Pa. on Sept. 19, McKeown said. Both were charged with murder in the first degree after they allegedly broke into Gklotsos' home the night of Sept. 17, then murdered him in a robbery gone bad, he said.
The Dover Police Department worked with local authorities in Pennsylvania towns to apprehend Lemonick and Newtown, McKeown said. Both were charged with murder in the first degree, home invasion, robbery, kidnapping and related offenses.
Gklotsos was murdered at approximately 10:30 p.m. that night, police said. By 10:42 p.m., Dover Police responded to a female caller who reported that she had been abducted from a residence in the 100 block of Acorn Lane and was released unharmed.
The woman told police that a man at the residence was assaulted during what she reported to be a home invasion. Dover Police Patrol Officers responded to the address in the 100 block of Acorn lane and discovered Gklotsos, 59 ,dead inside the residence.
The Delaware Office of the Medical Examiner determined that Gklotsos had been strangled.
Dover Police investigators knew a third person was involved in the break in based on what the female victim told police, McKeown said.
"We didn't know how she fit in," he said. "Through our investigation, we knew that she was involved. She left the residence prior to the homicide happening. We were able to identify her when we did our interviews in Bucks County, Pa."
Ferraro was later arraigned and remanded to the Stevenson House Detention Center in Milford in lieu of $64,000 secured bond.
Lemonick and Terek were extradited to Delaware on Monday, McKeown said. Lemonick was committed without bond to James T. Vaughn Correctional Center in Smyrna, and Terek was committed without bond to the Baylor Women's Correctional Institution in New Castle.
State law forbids bail for first-degree murder.


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Otro día más con los chicos.
Kawaii tattoos simple. 194 likes 7 comments kawaii tattoos kawaii tattoos on instagram. The adorable little cat has taken the internet by storm so naturally there are tattoos of her. It also includes sea life and other animals tattoos such as cute pets puppies kittens and horses to scary dragons flowers and fighting fish.
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How Massless Neutrinos Affect the Cosmic Microwave Background Damping Tail
We explore the physical origin and robustness of constraints on the energy density in relativistic species prior to and during recombination, often expressed as constraints on an effective number of neutrino species, . Constraints from current data combination of Wilkinson Microwave Anisotropy Probe (WMAP) and South Pole Telescope (SPT) are almost entirely due to the impact of the neutrinos on the expansion rate, and how those changes to the expansion rate alter the ratio of the photon diffusion scale to the sound horizon scale at recombination. We demonstrate that very little of the constraining power comes from the early Integrated Sachs-Wolfe (ISW) effect, and also provide a first determination of the amplitude of the early ISW effect. Varying the fraction of baryonic mass in Helium, , also changes the ratio of damping to sound-horizon scales. We discuss the physical effects that prevent the resulting near-degeneracy between and from being a complete one. Examining light element abundance measurements, we see no significant evidence for evolution of and the baryon-to-photon ratio from the epoch of big bang nucleosynthesis to decoupling. Finally, we consider measurements of the distance-redshift relation at low to intermediate redshifts and their implications for the value of .
High-resolution observations of the cosmic microwave background (CMB) temperature anisotropy are providing a precise measurement of the damping tail of CMB power spectrum, shedding light on the physical conditions during recombination and back into the radiation dominated era. The measurements have revealed somewhat less fluctuation power at small angular scales than expected in the standard cosmological model (Reichardt et al., 2009; Das et al., 2011; Dunkley et al., 2010; Keisler et al., 2011). Many papers (Dunkley et al., 2010; de Holanda and Smirnov, 2010; Fischler and Meyers, 2011; Krauss et al., 2010; Galli et al., 2010; Nakayama et al., 2011; Hamann et al., 2010; Keisler et al., 2011) have considered the possibility that this deficit of power is due to extra (dark) relativistic species 111Jungman et al. (1996) first pointed out that the number of species of relativistic neutrinos could be measured from CMB., such as nearly massless sterile neutrinos. Constraints are usually expressed in terms of an effective number of neutrinos, 222The effective number of neutrinos is defined so that the neutrino and photon energy densities are related by ..
Note that these constraints apply to any weakly interacting or non-interacting species that is relativistic at recombination. Hypothesized additional species include sterile neutrinos, sub-eV mass axions as in, e.g., Hannestad et al. (2010) and those arising in many other extensions of the standard model such as in Fischler and Garcia (2011).
Interest in the number of light degrees of freedom is further stimulated by i) recent inferences of the primordial Helium abundance which are larger, and with larger uncertainties than previous analyses Izotov and Thuan (2010); Aver et al. (2010, 2011), ii) evidence for additional (sterile) neutrino species from laboratory-produced neutrinos Aguilar-Arevalo et al. (2010) and reactor-produced neutrinos Mention et al. (2011) and iii) a slight tension between determinations of distance vs. redshift at very low redshifts (essentially measurements of Riess et al. (2011)) and those at low to intermediate redshifts that use the baryon acoustic oscillation (BAO) feature in the galaxy power spectrum as a CMB-calibrated standard ruler Mehta et al. (2012); Anderson et al. (2012).
Given this interest, and impending improvements to the damping tail measurements from the SPT (Keisler et al., 2011) (K11 hereafter) and the Planck satellite, a pedagogical exposition of the impact of on the CMB is quite timely. The relevant physics is beautifully simple and deserves to be as well (and as broadly) understood as the constraints on from big bang nucleosynthesis (BBN) considerations. Focusing on the physics behind the constraints also allows one to understand their more general implications. The only important assumptions about the relativistic degrees of freedom that go into the CMB predictions is that their interactions are negligible and they are massless.
Despite the analyses provided by Hu and White (1996) and Bashinsky and Seljak (2004) we find confusion in the literature about why increasing reduces small-scale anisotropy. The sensitivity to from high-resolution CMB observations is due to the impact of the mean relativistic energy density on the Universe’s expansion rate prior to (and during) the epoch of photon-baryon decoupling. As we demonstrate below, neutrino perturbations do not play a significant role 333An exception is the breaking of the degeneracy, to be discussed later., nor do anisotropies induced after decoupling. To demonstrate the insignificance of the early Integrated Sachs-Wolfe effect, we artificially introduce a scaling of its physical value by a parameter and examine the constraints on that follow from marginalizing over .
The constraints on are model dependent; there are other ways to extend the standard cosmological model to suppress small-scale power in the cosmic microwave background. We discuss, in particular, departures from a power law for the primordial perturbation spectrum, and allowing the fraction of baryonic mass in Helium, , to be a free parameter.
We also consider the sensitivity of inferences of from CMB data to assumptions about BBN and measurements of light-element abundances. Allowing to vary freely introduces a degeneracy that completely changes the mechanism by which is constrained by CMB data. We comment on the origin of constraints in the - plane.
In Section II we review the analytic explanation for the origin of constraints on from CMB observations and demonstrate its quantitative effectiveness in understanding constraints from current data. We also examine the model dependence of constraints on . In Section III we consider the impact of the early ISW effect on constraints and we discuss our results and conclude in Section IV.
Ii How CMB Observations Constrain Component Densities
Let us review the sensitivity of the CMB power spectrum to the densities today of baryons, , cold dark matter plus baryons, , and the dark energy, , all within the context of the CDM model 444Energy densities today are often expressed as, e.g., g/cm). For more details than we give here, see (Hu and Dodelson, 2002; Hu et al., 2001). In the course of our review, we will identify directions in parameter space that cause large changes in probability density. When we do study variations in we will do so along orthogonal directions.
ii.1 Sensitivity to the Non-neutrino Components
The dependence of the CMB on arises from the dependence of the equation-of-state of the pre-recombination plasma on the fraction of its energy density that comes from baryons. Increasing the number of baryons per photon decreases the plasma’s pressure to density ratio (). The resulting shift in the equilibrium point between gravitational and pressure forces alters the ratio of even peak heights to odd peak heights. We know the energy density of photons very well from measuring the CMB photon spectrum (Mather et al., 1990), and can thus infer from the ratio of even to odd peak heights.
The dependence on arises from the sensitivity of the evolution of a Fourier mode amplitude to the fraction of the energy density contributed by non-relativistic matter when the mode’s wavelength is equal to the Hubble radius. This ratio depends on where is the comoving wavelength, defines the comoving Hubble radius at the time when the matter density equals the radiation density (an epoch denoted by ‘EQ’) and is the scale factor parameterizing the expansion of the Universe. The amplitude of a mode projecting to angular scale depends on where because . Since the amplitude is a strong function of this ratio, there is strong sensitivity to and therefore to () since, assuming the dark energy is a cosmological constant, where is a very slowly-varying function of 555..
Thus the CMB power spectrum is sensitive to . If we assume the standard radiation content (, ), then a constraint on directly constrains . However, if we are allowing to vary, we should study its effects at fixed since this quantity is well constrained by the data. Prior to the CMB damping scale measurements, there were already hints of high by combining the constraint from WMAP with late-time observables sensitive to the matter density Komatsu et al. (2009).
We now consider . The angular scales of the acoustic peaks are highly sensitive to the angular size of the sound horizon, . Thus, is very precisely determined by the data. Given , we could infer . In a universe with zero mean spatial curvature, from the time of last scattering to today, and depends only on and . We do know , to some degree, from our determination of and as described above. These densities determine the history of the sound speed, 666 with and the expansion rate, allowing us to calculate since it depends on no other parameters in the six-parameter CDM model. This determination of allows for a constraint on .
ii.2 The Effect of Relativistic and Dark Degrees of Freedom
Changing only slightly alters the above story about the origins of the parameter constraints. We expect inferences of , and to be nearly unaffected. In the top panel of Fig. 1 we thus hold these parameters fixed while varying from 2 to 6. We hold fixed by increasing the density of cold dark matter as we increase . We keep fixed by changing to adjust .
As can be seen in Fig. 1, increasing along the chosen direction in parameter space, makes very little difference at low (exactly as intended) and an increasing difference at higher . A similar exercise was performed in Bowen et al. (2002), who identified the same parameters to be held fixed, but then ascribed the relative drop in power toward small scales as due to a post-decoupling effect known as the “early integrated Sachs-Wolfe effect.” This explanation was summarized and cited in Galli et al. (2010). We claim, in contrast, that these differences at high are almost entirely due to increased Silk damping, caused by the increased expansion rate. To demonstrate that the variation is not predominantly due to ISW, in the central panel we have normalized the spectra at where the ISW effect is negligible; we see that the high- variation is only slightly reduced.
Temperature anisotropies on scales smaller than the photon diffusion length are damped by the diffusion, a phenomenon known as Silk damping. Diffusion causes the drop in power toward high and makes the power spectrum sensitive to the angular scale of the diffusion length, . To second order in , where is the photon mean free path, the temperature fluctuations are suppressed by where the mean squared diffusion distance at recombination is
where is the number density of free electrons, is the Thompson cross-section, is the scale factor at recombination (defined below) and the factor in square brackets is due to the directional and polarization dependence of Thompson scattering (Kaiser, 1983; Zaldarriaga and Harari, 1995). Although Eq. 1 is only an approximation to the diffusion length, it allows an analytic understanding of the dependence of this diffusion length on model parameters (Hu and White, 1996).
If we approximate as independent of , then . This is as expected for a random walk process: the distance increases as the square root of time. Increasing (which happens when we increase ) leads to smaller which would decrease the amount of damping. Why do we see, in Fig. 1, the damping increase as increases?
The answer has to do with how and change to keep fixed despite the increased expansion rate. The comoving sound horizon is given by
Since , it responds even more rapidly to changes in than is the case for . To keep fixed at the observed value, must also scale as . Since decreases by more than would be necessary to keep fixed, increases which means the damping is increased.
To look at it another way, if we knew perfectly, we could use to determine prior to recombination. But we do not know , largely because we do not know the value of the cosmological constant, or more generally the density of the dark energy as a function of the scale factor. Instead, we can use the two scales together to form a ratio that is sensitive to , with no dependence on : .
Does this explanation hold together quantitatively? To demonstrate that what we are seeing in the power spectrum actually is increased Silk damping (at fixed ) we experiment with also fixing as increases. The bottom panel of Fig. 1 shows how the angular power spectrum responds to the same variations in , only now taken at constant as well. When we remove the variation, the impact of the variation almost entirely disappears. We conclude that the variations we are seeing in the top panel are indeed due to the impact of on the amount of Silk damping. A very similar demonstration was provided by Bashinsky and Seljak (2004).
To keep fixed as varies, we varied a parameter whose sole impact is on the number density of electrons: the primordial fraction of baryonic mass in Helium, . Even as early as times when 99% of the photons have yet to last scatter, Helium, with its greater binding energy than Hydrogen, is almost entirely neutral. Thus where the first equality defines and we have kept (and thus ) fixed. The limit of integration in the above equations for and is only slightly affected by changing and thus is largely unaffected. However, the damping length scales with as .
From our analysis one finds that where is proportional to . The first factor arises because increasing at fixed means . Thus as is varied, we know how to change to keep (and hence ) fixed.
However, the above analysis requires a small correction for two reasons. First, increased expansion, even if we keep fixed, decreases because we define , following Hu and Sugiyama (1995), such that the optical depth to Thomson scattering from here to is unity. Second, recombination is not a process that occurs in chemical equilibrium. As emphasized in Zahn and Zaldarriaga (2003), increasing the expansion rate leads to an increase in . By numerically studying these effects, which partially cancel each other, we find that with rather than 0.25.
Note that when varying in Fig. 1, we also vary as is expected for standard assumptions about BBN, as will be explained below. Following BBN consistency (as opposed to keeping fixed) increases the damping effect by about 30%.
We should mention that neutrino perturbations do alter the amplitude of the power spectrum at by a (nearly) constant factor Hu et al. (1995); Bashinsky and Seljak (2004). The breaking of the , degeneracy in WMAP data at low is due to the impact of neutrino perturbations, and this is the effect that allowed for an indirect detection of these perturbations as reported in Trotta and Melchiorri (2005); De Bernardis et al. (2008).
However, with the inclusion of small-scale data, the perturbations have lost their significance. In Fig. 2 we demonstrate that the constraint from WMAP + SPT is well approximated by combining the WMAP7 data with the information on from WMAP +SPT.
Fig. 3 provides another way of seeing the importance of to the constraint. From the color coding one can see that lines of constant run along the major axis of the probability contours. Further, one can see that the BBN consistency line cuts nearly perpendicularly across these lines. This feature explains why the errors on are about 30% smaller if one assumes BBN consistency rather than fixed . If we abandon BBN consistency and allow to vary freely, then is allowed to vary along the major axis of the probability contours and the constraint on loosens considerably, as described in more detail below.
ii.3 Constraining with free
We do not have a complete analytic understanding of the closing of the contours on the major axis (as opposed to the minor axis) in Fig. 3. We can turn though to the lowest panel of Fig. 1 to see that at fixed there is indeed some remaining variation to the power spectra as varies. At least some of this variation is due to the difference in acoustic oscillation phase shift that one gets for neutrinos, relative to the same energy density in photons, due to their free streaming Bashinsky and Seljak (2004).
Another effect important for breaking the degeneracy between and is due to high baryon fraction. In our above analysis we assumed that is a fixed constant. However, this assumption will break down when decreases to lower values, as it can do if is allowed to vary freely, while the baryon density remains unchanged. As decreases, to keep fixed, would decrease, thus driving up the baryon fraction, . Effects due to the high baryon fraction make it impossible at sufficiently low to find a value of , and that reproduce the measured power spectra. In an attempt to best accommodate the data, the region of high likelihood departs from constant , as can be seen in the upper panel of Fig. 4 which shows probability contours in the - plane. The lines are lines of constant and . As extra freedom is allowed in the model, allowing to extend to lower values, we can see the expected departure of the probability ridge from the line of constant and , mainly due to variation of .
A high baryon fraction alters the acoustic dynamics for modes entering the horizon during matter domination, because a large fraction of the matter sourcing the gravitational potentials is feeling pressure support. This pressure support causes potentials to decay, boosting the amplitude of the fluctuations as happens with the “radiation driving” in the radiation-dominated era. At fixed , increasing boosts the height of the first peak relative to the second. The existence of this radiation-driving-like effect in the matter-dominated era impacts the ability to constrain . One can see in the lower panel of Fig. 4 how the uncertainty in increases when is allowed to take on smaller values (as happens when allowing to vary freely). The effect is even greater when allowing further freedom in the model by allowing to vary, a parameter we will introduce below.
Iii Constraints on
Here we present constraints on from current data. We begin with our baseline estimates, which are from CMB data alone, assuming the six-parameter CDM model extended by one to allow free , with determined by a BBN consistency relation to be discussed below.
We also consider departures from our baseline assumptions. We let vary away from the standard BBN relationship, let vary away from what is expected from inflation and allow the early ISW effect to be greater or smaller than expected, by introducing an artificial scaling parameter, .
Finally, we consider the influence of low-redshift distance measurements on inferences of .
iii.1 Baseline Constraints
The PC superscript indicates the Pettini and Cooke (2012) inference, A indicates Aver et al. (2011) and P indicates Peimbert et al. (2007). The difference , and .
iii.2 Sensitivity to BBN Assumptions
The standard assumption is that the baryon-to-photon ratio and are unchanged from BBN through decoupling. However, many processes can change this situation, such as energy injection into the plasma after BBN which would reduce both and , or a decay of a massive dark species into a relativistic dark species after BBN, which would increase while leaving unchanged. Here we relax the standard assumption and distinguish the variables with superscripts DEC (for decoupling) and BBN.
First we consider the extreme of making no assumptions about BBN and using no light-element abundance data to constrain the BBN quantities. In practice this simply means allowing to be free. As one would expect from our earlier discussion, allowing to be a free parameter greatly relaxes the constraints on because of its impact on . This is shown in the second row of Table 1.
If we assume standard BBN, we can use measurements of the abundance of Deuterium relative to Hydrogen, , and to determine and . Simha and Steigman (2008) provided fitting formulae for the dependence of and on these quantities. Here we present revised ones 777G. Steigman, private communication, that incorporate updates in nuclear reaction rate estimates and a neutron lifetime estimate. They are
To calculate as a function of and we use the default CosmoMC option which is an interpolation over tables produced using PArthENoPE v1.00 described in Pisanti et al. (2008), only using Eq. 3 for values outside the bounds of the tables for robustness but very rarely reached. To calculate we use Eq. 4.
For the measurements of light element abundances we mostly follow Nollett and Holder (2011). They assumed, from a compilation of measurements (see Pettini et al. (2008); Fumagalli et al. (2011) and references therein)
We also consider a very recent, and significantly more preicse, measurement by Pettini and Cooke (2012) of
Note that signifcant uncertainty arises from nuclear reaction rate uncertainty. When using measurements we include the 6% error in Eq. 4 and add it in quadrature with the measurement error.
For Helium Nollett and Holder (2011) considered two different inferences
Including the light element abundance measurements to help constrain reduces the uncertainty in , though it remains comparatively large. Interestingly, the lower measurement, which is the only one of the two consistent with , leads to a slightly higher inference. This is because lower values need higher to get the same .
Pettini and Cooke (2012) took an inference of the baryon density from Keisler et al. (2011), calculated assuming , combined it with their measurement, and the above fitting formula, and found . Thus they show that their data are consistent with the combination of CMB data and the assumption of .
We performed a similar, but different, exercise where we set and estimated both values simultaneously from the CMB and D/H data. There is a small correlation between and as inferred from the CMB data which leads to increased inference when is allowed to vary. The net result is that our exercise leads to a higher value, , with .
We note that our analysis, in which we allow the BBN quantities to be different from the DEC quantities, is for a very general scenario and thefore missing features that may be important for specific scenrios. For example, in Eggers Bjaelde et al. (2012) a scenario was considered in which increases after BBN due to the decay of a fraction of the dark matter into dark radiation. With such a specific choice, one can include in the calculation the details of how this conversion happens over time, and the differences in the dark radiation perturbations from the case of thermally produced neutrinos.
iii.3 Sensitivity to primordial power spectrum assumptions
Another straightforward way to reduce small-scale power is to alter the primordial power spectrum. For the usual power-law assumption, the exponent is sufficiently well determined by low- data that it cannot mimic the damping effect of . However, if we allow for to have a logarithmic scale dependence so that for some constant then the resulting power spectra can better mimic the effects of . As a result, if we marginalize over , we increase the uncertainty in , as can be seen in Table 2.
iii.4 Importance of the early ISW Effect
The anisotropy field today can be written as an integration over perturbation variables on the past light cone. Doing so can be useful both computationally (Seljak and Zaldarriaga, 1996) and for analytic understanding. Writing the Fourier and Legendre-transformed radiation transfer function as such an integral (ignoring the polarization-dependence of Thomson scattering for simplicity) one gets
See Dodelson (2003) for definitions. The final integral is the so-called integrated Sachs-Wolfe (ISW) effect. The other terms are only important when the visibility function, is non-zero, whereas the ISW term gets contributions along the whole line of sight between here and recombination where starts to get very large. The gravitational potential time derivatives are zero for a Universe dominated by cold dark matter. They are significantly non-zero at early times as the radiation density is still a significant contributor to the expansion rate (the early ISW effect), and then again at late times when dark energy becomes important (the late ISW effect).
In Eq. III.4 we have introduced the parameter so we can artificially vary the amplitude of the early ISW effect. The function when the redshift, and otherwise equals one. This use of is very similar to the use of to artifically change the amplitude of the lensing potential power spectrum altering the CMB power spectrum. We might have chosen to go as the square root of so that is scaling the ISW power (just as scales up the lensing power). However, a significant impact of the ISW term in Eq. III.4 comes from its correlation with the other terms in the equation. Thus there is no way to make the total contribution of eISW to the power scale as a single power of .
The greater the amount of radiation around, relative to matter, at recombination, the greater the amplitude of the early ISW effect. Thus increasing (with held fixed) would increase the amplitude of the early ISW effect. This relationship between and the early ISW effect led Bowen et al. (2002) to cite the ISW effect as the reason the CMB is sensitive to .
To quantitatively investigate the impact of the ISW effect, we could perform the exercise of turning it off artificially. But turning off the ISW effect would so radically change the first peak (dropping it in power by 28%) that we instead chose to investigate by letting be a free parameter. If the ISW effect is playing an important role in constraining then if we let it be a free parameter, those constraints will degrade and we will also see a strong correlation between the two parameters.
We show probability contours in the - plane in Fig. 5 for the case that follows the BBN-consistency relation and the case that is free. For the BBN-consistency case, the constraint on degrades by less than 10%. But when is allowed to vary freely, the constraint can no longer determine because of the degeneracy with . In this case, the region of the spectrum affected by ISW is more important for determining so we see a significant degeneracy between and .
We also see from Fig. 6 that marginalizing over does little to expand the minor axis of the contours. As we have emphasized, the constraint along this axis is due to the constraint on . Along the major axis the ISW effect does play a role in breaking the degeneracy. Other effects important in breaking this degeneracy include those coming from neutrino perturbations (Bashinsky and Seljak, 2004) and high baryon fraction as discussed in Section II.3.
Iv Implications for Low-redshift Distance Measurements
We now consider the implications of CMB measurements, in the context of variable , for low-redshift measurements.
First let’s consider the effect on the expansion rate at low redshift for the CDM + cosmology. Increasing , with the resulting increase in (to keep fixed) increases the expansion rate through the matter-dominated era. Further, in order to adjust to keep fixed (given the decrease in ), the energy density in the cosmological constant, , must increase as well. With the energy density in both components important at low redshift increasing, increases for all redshifts in the low-redshift (matter-dominated and later) regime.
Note that if we can ignore changes to the limit of integration in Eq. 2 then we expect . With this scaling, we then expect to keep fixed. The only way to achieve that scaling in the CDM model is to have the dark energy density scale in exactly the same way as . Hence , and therefore scale the same way at all redshifts. If also has no variation with then the net result is that the BAO observables and have no dependence on . Note that is the epoch of photon-baryon decoupling defined as in Meiksin et al. (1999).
In practice there are many corrections to the above analysis, e.g., the correlation between and , but they are all small and the net result is very little dependence of the BAO observables on . We can see that in Table 2, where adding in just BAO data makes very little difference to the inference. Another consequence of scaling similarly as is that does not scale with .
Fig. 8 quantitatively supports the above discussion. We compute the quantity at the redshift where the latest BAO data were effectively measured (Anderson et al., 2012). We see that , ; i.e., they both scale nearly as . And their scalings are so similar that the ratio of the two quantities shows no noticeable correlation with . In the case of WMAP7+K11+BAO+, we get , compared to in K11 (Keisler et al., 2011) for our baseline model. The only difference comes from the latest BAO data point which shows a little tension with the inference from the CMB data888Note that Anderson et al. (2012) report for an given by the fitting formula of Eisenstein and Hu (1998). We have adjusted the reported value for comparison to calculated with our definition of by multiplying it by 154.66/150.82. See Mehta et al. (2012).
What is sensitive to at low redshift are absolute distance measures that are not calibrated with . The inference of , given CDM (with standard radiation content) calibrated with the WMAP7 and SPT data is . This is 1.17- lower than the Riess et al. 2011 value of (Riess et al., 2011). Increasing to the higher value preferred by the CMB data alone brings these two inferences into better agreement. One can see the impact of the Riess et al. measurement on the reduced uncertainty in in the Table entries for the CDM + cosmology; including the Riess et al. measurement drops the uncertainty by about 50%.
Varying thus changes the CDM, CMB-calibrated predictions for , without much change in the predictions for the BAO data – consistent with the analysis in Eisenstein and White (2004). Increasing thus can eliminate the tension between the BAO data and the Riess et al. measurement as pointed out in Mehta et al. (2012).
The case of free allows us to see this preference of the low-redshift data for the that comes from an increased . With CMB data alone, letting the running vary leads to a downward shift in the central value for . Adding in the and BAO measurements shifts the preferred value for back up towards 4.
Increasing also has implications for the growth of structure. Increasing leads to an increase in which in turn decreases . Decreasing the baryon fraction decreases the pressure support felt by matter prior to recombination, thereby boosting the growth of structure on scales smaller than the sound horizon at recombination; i.e., scales smaller than about 150 Mpc (Eisenstein and Hu, 1998). Therefore increasing increases cluster abundances, that are sensitive to the power spectrum amplitude on 10 Mpc scales. This effect can be seen in joint estimates of (which has the opposite impact on small-scale power) and from cluster abundances in Benson et al. (2011) and also in Hamann et al. (2011).
There are several ways that massless neutrinos impact the anisotropy of the cosmic microwave background. Here we have shown that current CMB constraints on are dominated by the impact of the neutrino energy density on the expansion rate. Although is sensitive to this change in expansion rate from , its simultaneous sensitivity to the distance to last scattering greatly limits how well can be reconstructed from it alone. Measuring the damping tail region has allowed a measurement of as well. Since the response of to the expansion rate is different from the response of , their ratio (which is independent of the distance to last scattering) is sensitive to the expansion rate.
The above analysis assumes that follows the BBN consistency relation. Since also alters , allowing it to vary freely introduces a near degeneracy between and . This near degeneracy is broken by a number of physical effects at low , including the early ISW effect and effects of a high baryon fraction. At high the acoustic oscillation phase shifts probably play an important role, although we have not quantitatively confirmed this hypothesis.
We defined a phenomenological scaling parameter of the early ISW effect, . We used it to show that the ISW effect plays a very small role for the case of BBN consistency, although, as just noted above, it does contribute to constraints on when is allowed to vary freely. We found that, assuming BBN consistency, – a highly significant (though model dependent) detection of the early ISW effect.
We tested the consistency of inferences of , and from CMB data, with inferences from light element abundance measurements and BBN theory. We see no strong evidence for any inconsistency, though the bounds are quite loose. For the most discrepant case we find . We note that a simultaneous inference of and from the CMB and the new Pettini & Cooke D/H measurement results in an more consistent with 4 than is the case for the similar exercise performed in Pettini and Cooke (2012).
We considered the impact of low-redshift distance-redshift relation measurements on determination of . We found that BAO data are not very sensitive to because and scale similarly with . The same cancellation does not occur for distance measures that calibrate independent of the CMB, such as the Hubble constant determination in Riess et al. (2011).
We will have tighter measurements from the forthcoming analysis of the entire SPT survey, and we expect improvements to come from Planck in early 2013. We project that the error on will reduce to 0.33 using simulated full-survey SPT data combined with existing WMAP and data, and will reduce further to 0.20 using simulated Planck data and existing data, assuming the Planck data and foreground model of Millea et al. (2011), consistent with the forecasts of Bashinsky and Seljak (2004) and Hannestad et al. (2006).
Acknowledgements.We thank A. Albrecht, B. Benson, O. Doré, E. Komatsu, M. Luty, J. Ruhl, L. Strigari, A. Vikhlinin and M. White for useful conversations. We acknowledge support from NSF awards no. 0709498 and ANT-0638937. We used CosmoMC (Lewis and Bridle, 2002).
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"Justice wears a green hood." The series premiere of Arrow is slated for Wednesday, Oct. 10 on The CW.


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