The name is familiar except you are new around here. Gabriel Afolayan has been a prominent actor and has taken parts in countless soap operas on TV and home videos but he shocked many recently when he released a love song titled 'Kokoro ife'.
The release of the song has been dubbed a commendable one from the first timer; known for his role in movies.
Gabriel who is under Studio 6 is determined to prove a point and go beyond borders with his 'Kokoro ife' love song which will be followed by a new single and an already made video shortly. Ace producer Masterkraft made the beat. The song is a single off his yet to be titled album.
Gabriel Afolayan who is also known as G-Fresh however is not bidding his acting career farewell. On Saturday, he bagged the 'Best Actor in a Supporting Role' and The 'Rising Star' awards in the highly rated Nollywood Movies Award (NMA) and 'Most Promising Actor'award at the 'Yoruba Movies Academy Awards' in Abeokuta, Ogun State the next day.
The theatre arts graduate of the University of Ibadan has featured in several movies and soap operas including a supporting role in 'Ghetto Dreamz', the movie that spotlights the life of Dagrin the late rapper and Tade Ogidan's 'Madam Dearest'.


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First Annual Tigua Inc. & Tigua Transportation Golf Classic Benefits Muscular Dystrophy Association
Local CITGO Lubricants Marketer Raises Funds for El Paso Families Living with Neuromuscular Disease
Thursday, December 19, 2013 - 9:30am
CAMPAIGN: CITGO Station Owners and Operators Committed to Giving Back to Their Communities
EL PASO, Texas, Dec. 19, 2013 /3BL Media/ -- Local CITGO Lubricants Marketer/Distributor Tigua, Inc. and Tigua Transportation joined forces with the Rio Grande Chapter of the Muscular Dystrophy Association (MDA) to launch its 2013 Inaugural Golf Classic on Oct. 28, 2013. Sixty-five members of the El Paso community gathered at Butterfield Trail Golf Course to raise money in support of the local chapter of MDA. The funds raised this year stay in the El Paso area to repair durable medical equipment items, support group sessions and local clinics, fund ongoing research and send local children to MDA summer camp.
"We are pleased to start this annual tournament to benefit MDA," said John Baily, CEO of Tigua, Inc. "There is so much work to be done in the field of neuromuscular disease, and we are happy to be doing our part to help those impacted by muscular dystrophy. The results this year are a great jumping off point that we can continue to grow year after year."
The October tournament served as the first step toward an annual tradition of supporting the El Paso MDA chapter and included some very special guests this year. The participants had the privilege of playing with five soldiers as part of the Better Opportunities for Single Soldiers (BOSS) program. BOSS, which works to enhance quality of life for soldiers that are on their own, helps soldiers identify and plan leisure activities and encourages participation in community activities like local fundraisers.
"This golf classic is off to a great start and we can't wait to see the good that future tournaments will fuel," said Karl Schmidt, general manager petrochemicals and lubricants with CITGO Petroleum Corporation. "We are proud to be part of events that raise funds for MDA, and to be part of this tournament as it provides an opportunity for community members, including those who serve our country, to gather for a worthy cause."
Tigua, Inc. is tribally owned by the Ysleta del Sur Pueblo (YDSP) "the Pueblo," a U.S. federally recognized native American tribe and sovereign nation. It is a holding company for five subsidiary companies with Tigua Transportation being one of them. Tigua Transportation serves as the main distributor in the El Paso area for CITGO.
CITGO is the largest corporate sponsor for MDA, raising more than $160 million over the last 27 years through the generosity of its employees and its network of locally owned Marketers and Retailers, like Tigua Inc. CITGO supports local events like the Tigua Inc. & Tigua Transportation Golf Classic, as well as the CITGO Fueling Good Project, which recognizes local heroes and the good works they do in their communities. To learn more about Fueling Good and how local organizations are making a difference, please visit www.FuelingGood.com.
CITGO Lubricants manufactures a wide range of oils, fluids and greases for use in on-road and off-road fleets, equipment and vehicles as well as agricultural, industrial gas, metalworking and railroad applications. The company offers customized lubricant solutions that improve productivity and efficiency and these products are available through local and regional distributors and at CITGO Fast and Truck Lube locations. For more information, visit www.citgolubes.com or call 1-800-331-4068.
SOURCE CITGO
For further information: Eleanor Rutland, 202-973-1313
CATEGORY: Events, Media & Communications

redpajama_set_name: RedPajamaCommonCrawl


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Author: Kenneth Loh 羅健晃
Dr. Kenneth Loh is an Associate Professor in Civil Engineering at the Nano-Engineering and Smart Structures Technologies (NESST) Laboratory at the University of California, Davis. He received his Ph.D. in Civil Engineering from the University of Michigan. He conducted his Fulbright research in bridge scour monitoring at National Taiwan University. His research interests include multifunctional materials and resilient structures.
Smart Sensors for Safer Bridges: An International Collaborative Effort
Kenneth Loh 羅健晃 February 24, 2015
Bridge Scour The erosion of soil, sand, and riverbed materials near bridge foundations due to flowing water (or wind in some cases) is a phenomenon known as bridge scour. Despite our awareness of its occurrence, bridge scour remains one of the deadliest causes of overwater bridge failures worldwide, particularly in the United States and in Taiwan. For instance, a notable scour-induced bridge collapse in the United States was the Schoharie Creek Interstate Highway Bridge incident in Mohawk River, New York, which happened in April 1987. The 32-year-old bridge collapsed due to extensive flood-induced scouring at one of its piers, and 10 people lost their lives. In Taiwan, similar incidents have occurred as well. More recently in September 2008, Typhoon Sinlaku brought heavy rainfall across many parts of Taiwan. The Houfeng Bridge collapsed due to flooding and severe scouring near one of its piers, although it was suspected that long-term riverbed degradation following the Chi-Chi earthquake in 1999 also contributed to its failure. Events like these could be traced back through the histories of both countries. Even worse is that overwater bridge collapses after scouring continue to occur and threaten public safety. The inability to


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The 2009 AdvoCare V100 Independence Bowl was the thirty-fourth edition of the college football bowl game, and was played at Independence Stadium in Shreveport, Louisiana.  The game started at 5:00 PM US EST on Monday, December 28, 2009. The game was telecast on ESPN2 and the Georgia Bulldogs defeated the Texas A&M Aggies by a score of 44-20.

The game was Georgia's second appearance in the bowl game. Their previous appearance in the game was a 24–15 victory over the University of Arkansas in 1991.

As for Texas A&M, the Aggies made their third appearance in the Independence Bowl and now hold an overall record of 1–2. Their last appearance resulted in a 43–41 overtime loss to Mississippi State on December 31, 2000, a game since nicknamed the "Snow Bowl" due to the unusual amount of snowfall Shreveport received that day. The entire game was played under extremely wintry conditions, a rarity for Shreveport.

The game was the fifth time that the two schools have faced each other in a game.  Texas A&M previously held the series advantage 3–1 (now 3-2). The last time, prior to the bowl that the two teams met was a 42–0 victory by Georgia in 1980. The two teams have played in a bowl game against each other once before, as they met in the 1950 Presidential Cup Bowl. The game, which was played in College Park, Maryland, was the only ever edition of the Presidential Cup Bowl, and Texas A&M was victorious by a score of 40–20.

Game summary
Georgia wore their home red jerseys, and Texas A&M wore their away white jerseys.

Georgia's quarterback, Joe Cox, threw for 157 yards and two touchdowns as the Bulldogs dominated Texas A&M to win their fourth straight bowl game.  Tight End Aron White caught both of Cox's touchdown passes, one from 24 yards out and the other a two-yard catch, on his way to being named the game's offensive MVP.  Caleb King paced the Bulldogs rushing game with 61 yards on 16 carries and two touchdowns.  Special teams also played a huge part in the Georgia victory.  The Bulldogs scored their first touchdown of the game on a kickoff return for a score.  Georgia also blocked a punt and a field goal attempt, and recovered a bad snap on a punt at the Texas A&M 24-yard line.  Aggies quarterback Jerrod Johnson passed for 360 yards and two touchdowns, but also threw two costly interceptions.  Jeff Fuller led A&M with 7 receptions for 101 yards in the losing effort.  Georgia's six touchdowns tied an Independence Bowl record. And Georgia's 30 second-half points established a new record for points scored in a half for the Independence Bowl.

Scoring summary

References

Independence Bowl
Independence Bowl
Georgia Bulldogs football bowl games
Texas A&M Aggies football bowl games
December 2009 sports events in the United States

redpajama_set_name: RedPajamaWikipedia


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Privatising Aer Lingus
I watched the weekly political debate show, Questions & Answers, last night. It confirmed all my worst fears about the corporatisation of politics. You've no idea how much it annoys me that the field of debate has been so narrowed; that mainstream politics has been reduced to a few ever-so-slightly differentiated shades of capitalist grey. The politicos on the panel were a Labour TD (TD = MP) representing the left, a government minister representing the centre, and an independent Senator representing the right.
The first question asked whether or not the privatisation of Aer Lingus "represents a good deal". Now, it's only since I've returned to Dublin that I realised Aer Lingus (Ireland's national airline) was still state-owned. Not only that, but it is currently – relative to its size – an extremely profitable airline. In the past, during downturns in air travel or during periods of mismanagement, the company has required government / taxpayer support. Now that it is doing well, the current government (plus the main opposition party) think it's a good idea to sell it off.
Presumably the idea is to make some quick cash on the deal before peak oil wipes out the airline industry. And regular readers might think I'd be in favour of that… offload an asset soon to become damn near worthless into the hands of a bunch of market speculators. Use the money to build a few hospitals. What could be wrong with that? Well. Quite a lot actually.
Am I never happy?
Well, yes. But not when a bunch of centre-right oafs are blundering around the country, selling off any public asset that isn't nailed down. I once wrote that I believed Britain could still be defined, loosely, as a socialist nation up until Thatcher sold off the energy and communications infrastructure. By doing that she made a bunch of money for the already wealthy and ended the ability of the British public to control their own economy.
Recently this Irish government has flogged the telecommunications system, converting its legal status from "service provider" to "profit engine". It's interesting to note that investors are very happy with the deal, but the Irish citizen is less so. Leastways that's the portrait painted by the media. Thankfully it looks as though energy production will remain public at least until capitalism begins to visibly decay (and hence, indefinitely). So Ireland is – in a specific, but very real sense – still socialist to a degree. As of right now, the public still owns significant assets, significant elements of the economic infrastructure and can exercise control over those assets through their democratic representation.
Few things piss me off more than watching politicians; the peoples representatives; shake their heads and meekly (or even worse, condescendingly) state that they can't do anything about a social problem because it's in the hands of private enterprise. For years successive British transport ministers agreed that the rail system was deteriorating, but told the public that they had no control over the way private companies are run. It makes me want to wring some necks.
Which brings me back to Questions & Answers and the subject of privatising Aer Lingus. The very first thing that should be pointed out is that this is a godawful deal. Even if I dust off that capitalist hat I tried on for size back in the 90s, the fact is – if you were going to privatise an airline, you really wouldn't do it this way. The government intends to retain a significant, but minority shareholding in the company. This means there's a siginificant reduction in the amount of shares being sold, and a consequent loss of income. On top of that, by retaining an influence on the company board of directors, it makes the whole airline less attractive to private investors who will worry about "government meddling" and fear that they won't be able to make the business as profitable as they would like if it was required to go against the policy of the government of the day in order to do so (a government that could be Green or Leftist or anything in 10 years).
So essentially; from the point of view of the taxpayer, the government is nigh guaranteeing the lowest possible price while at the same time ceding control over the asset. And from the point of view of the capitalist, the government is retaining the right to interfere with how a private company is run, and thus making the whole venture far less likely to succeed commercially. On top of all that, the newly privatised company intends to borrow at least as much as it earned from the floatation as soon as privatisation is completed. Possibly significantly more. All of which reduces the price that investors are willing to pay for those shares that are made available.
Given the likely direction to be taken by the airline industry in the face of peak oil, this will result in the collapse of the privatised Aer Lingus within about 10 years. Probably less given how deeply in debt they will be. And there'll be very little the government will be able to do about it, except wait until the company runs itself into a massive mountain of debt and bail them out at an absurd cost to the exchequer. Far, far more than was gained in the sell-off.
But hey, I've no doubt a bunch of already-wealthy speculators will make a small fortune in the immediate aftermath of the privatisation. So that's alright then. Once the government looks after them, the average citizen can rest easy knowing he or she only has to become a millionaire and they too will be represented by the people they vote for.
Market disengagement instead of privatisation
What should be done is obvious. Market disengagement. And what annoyed me about Questions & Answers was the fact that not a single member of the panel even hinted at having thought in these terms, let alone giving them the headspace to examine seriously. The Labour TD was opposed to privatisation, as are her party. Credit where it's due. However her objections were all about practical issues. It's as though the notion that there may be an ideological debate to be had was somehow quaint. Faintly embarrassing. You got the feeling that perhaps she had convictions, but wouldn't dream of admitting that in public… so if you could demonstrate that "the deal was good" for the taxpayer that all would be well.
She even resorted to the bland buzzwords of doomed capitalism. About how "everyone wants to see" Aer Lingus compete well in the marketplace. About how "of course" we want to see the company grow and expand into new routes and markets. Sheesh… doesn't anyone actually believe anything anymore? I mean aside from The Race For Profit Is A Race That Must Be Won.
I was reminded of Douglas Adams' wonderful observation about the BBC…
Television companies are not in the business of delivering television programs to their audience, they're in the business of delivering audiences to their advertisers. (This is why the BBC has such a schizophrenic time – it's actually in a different business from all its competitors)
Douglas Adams | What have we got to lose?
You see, it is my belief that a state airline should not be trying to "compete" at all. In the marketplace or anywhere else. It should be run, like any other state asset, in a manner that can best serve the Irish public. Everyone on the panel, and – it seems – everyone in the Irish media, believes that Aer Lingus needs significant new investment to buy more planes so that it can expand. But that's complete nonsense. It is not the best way to serve the Irish public. The last thing Aer Lingus should be planning is expansion.
Look, the airline business is at its peak right now. Maybe another two years… maybe three tops. After that, it's permanently downhill for jet-engined passenger flight. But I accept that whatever commercial flight does still exist during the next 10 or 15 years will look something like its present form. There'll just be a lot less of it, and it'll be much more expensive. Eventually it'll die completely and all international flight will be done in slow solar-powered dirigibles, and the enterprise will become rather sedate and civilised, with dining rooms and cool observation decks and everything (that's the optimist talking… I usually keep him locked in the cellar).
But until then, and while modern air travel is gasping its last, there will remain a need for scheduled flights to and from this country. It is the job of a state airline to provide that service as effectively as possible. It is not its job to compete with other airlines in the lucrative low-cost short-haul market. Nor its job to expand into another five US destinations and provide the Irish consumer with more choice. Its job is to ensure that Irish people can get to and from wherever they need to go, whenever they need to go there. That this island does not become isolated before anywhere else. Climate change activists may not like this job, but all the same, that's what it is.
And to this end, the best strategy is to begin reducing the size of the company and securing its ability to do two things very very well. Getting people to and from Heathrow efficiently. And getting people to and from New York efficiently. From Heathrow there are connecting flights to every major city in the world. From New York, to everywhere in America.
Over a period of a couple of years, Aer Lingus should sell off its entire fleet with the exception of those aircraft required to service New York and London. This would almost certainly (bizarrely) net the government more than the sale of the company as a whole. Of course, the workforce and the unions won't like that very much. And that's where the traditional left is really coming from with its desire for expansion.
But look, these are well-trained professionals by-and-large and they'll be beating the rush. The entire industry is going to be shedding jobs before too long; let the Aer Lingus staff get that particular skillset into the job market before the others. And by losing their jobs because of a deliberate scale-down and asset sale, they can get very generous redundancy cheques; unlike those who lose their jobs through bankruptcy. The rest of the money from the asset sale (planes cost a lot of money, I'm sure there'll be some left over) can make up the current pensions deficit in the company.
Those two routes alone may not make a profitable company. I honestly don't know. But even if it didn't, I'm certain it could be done efficiently enough so that the shortfall in the running costs won't cost the taxpayer too much. And in return for that small tax burden, Irish people know that they are securely connected to the rest of the world via a service they themselves own and control. At least until either Heathrow or New York cease fulfilling their function due to peak oil… but I guarantee you that a privatised Aer Lingus will go under before that happens.
Capitalists will complain of course. Blah blah blah government subsidies blah blah blah restrictive practices unfair competition blah. And yes. It's all those things. Even the blahs. What part of "anti-capitalist" don't you understand? But hey, just think of all the fun the other airlines will have fighting for scraps… expanding into the routes abandoned by Aer Lingus… after all, if Aer Lingus is selling the planes, someone is buying (and it's a little known fact that there's a shortage of commercial jet aircraft in the market at the moment… airlines are placing big orders and having to wait years for delivery… right now, it's a sellers market).
Many on my side of the barbed wire may be looking at me a little askew also. Am I trying to put forward some kind of sustainable jet airline industry idea here? Preaching business as usual? Isn't that precisely what I criticise the mainstream environmental movement for doing? Well yes, that is what I criticise the Greens for, but no that's not what I'm doing.
If tomorrow I were ordained God Emperor, then it'd be solar-powered dirigibles or nothing. So get those thinking caps on over at JPL, you folks are very very smart, I've no doubt you can adapt to a new specification and come up with some wild new ideas. The reality is, whatever way you cut it, the airline industry – in its current form – will not survive.
However, what would I do in the unlikely event that I'm not made God Emperor, but instead merely put in charge of Aer Lingus and given a specific brief… "Turn this profitable company into a public service and ensure that Ireland is connected to the international transport network so long as that network exists".
And well, that's what I'd do.
Posted in: Opinion
Economics Ireland Peak oil Public Transport
5 responses to "Privatising Aer Lingus"
[…] Meanwhile the Irish government have announced that Aer Lingus, the national airline, will be floated on the stock market by the end of September. As I've discussed previously, this is an idiotic decision made by greedy politicians who simply don't understand the concept of public service. Capitalists, fools and self-interested scoundrels to a person. A pox upon them all. […]
August 28th, 2006 | 3:06pm
by The Quiet Road » Blog Archive » Stuff
Sorry but I do not agree with all this state run public service stuff . Public service organisations end up as a job clubs to serve the interests of the employees . The customers and the public are ignored. The employees inside state monopolys just end up screwing the tax payer .Result lousy services , bloated terms and conditions etc etc . Look at Bus Eireann and Irish Rail . A joke . Privitise the lot of them , bring in competition , and lets have excellent services delivered by the private sector with suitable state regulation . I am afraid your nirvana will never happen . Just look what happened in the old USSR when they tried to get the state to run things . It does not work . Wake up and smell the roses . Socialism does not work . Get over it . End of story .
September 20th, 2006 | 6:15pm
by Eamon
It's interesting, Eamon, that you choose the obviously worst cases of state run industries as your examples. And then conclude from your self-selected data that functioning public services are part of a "nirvana" that "will never happen".
You go on to champion the private sector. But if we're going to have an honest debate, then we need to compare like for like. Right? I mean, I assume it's an honest debate you want and not a dogmatic slanging match.
So if we are to assume that the "old USSR" equates to socialism in action, then what should we consider an equivalent example of private capital in action? Enron? Union Carbide? Railtrack PLC? British Nuclear Fuels PLC? Can we assume that the Shell Corporation's actions in the Niger Delta is representative of private capital?
I think you'll find that you haven't presented a coherent argument against public ownership, merely against the bad implementation of it. I'm not suggesting that we run public services badly; no more than your suggestion that we "privatise the lot of them" is asking for them to be run like Railtrack.
If you do actually have a coherent argument against my position on Aer Lingus then I'd love to hear it. But claiming that it's better to run things like Enron rather than like Bus Eireann doesn't seem all that relevant to me.
by Jim
Yes, but Jim you haven't woken up and smelled the the roses. I'm afraid that's where Eamonn has got you.
September 21st, 2006 | 12:39pm
by Larry Teabag
[…] Privatising Aer Lingus (redux) October 5th, 2006 | 1:24pm by Jim Y'know, way back in April I argued that privatising Aer Lingus was an absurd idea. It would essentially be trading an important public asset for a small increase in wealth for the already wealthy. Aer Lingus was a successful public service, doing roughly what the people of Ireland needed of it. It was under our control and had a legal obligation to serve our needs. How could we possibly expect to improve on that by putting it under someone else's control and giving it a legal obligation to serve their needs? […]
October 5th, 2006 | 1:24pm
by The Quiet Road » Blog Archive » Privatising Aer Lingus (redux)
Comments have been closed on this post to prevent spam. If you wish to add a comment, however, simply post it to a more recent entry along with a note about where it should go. I'll reopen the comments here and transfer it over.
Join up your thinking, Mr. McWilliams
On hearing the news from Greece
An aggressive response to tyranny
NIMBYism
Food miles. More complicated than you may think.
Green Party support for BioFuels [updated]
Privatising Aer Lingus (redux)
Frances Fitzgerald: candidate for The Man
Biofuels – The fuel of the future


One hundred years old? You barely look a day over 99! Stop by the Public Health Expo and say "Happy 100th Anniversary" to members of the Health Administration and Statistics Sections, whose booths are in the Sections area of the expo.
The Statistics Section, top, hands out celebratory cupcakes, and the Health Administration Section, bottom, greets a booth visitor.


text:
Q: The video is played backwards, and the picture is choppy. With hls I want to play backward the video. But I found that the picture is choppy. As the picture below (the current time is change, but the picture not change. And after some time, picture change.)
<template>

    <video ref="videoRef" controls width="400px"></video>

    <button @click="play">Play</button>
    <button @click="pause">Pause</button>
    <button @click="windback">Windback</button>

</template>

Anyone have some advices?

redpajama_set_name: RedPajamaStackExchange


So I recently got my hands on a Sennheiser MK4, and decided to put it through its paces. I decided to do a "shootout" comparison with an AKG 414. I'm including the sound clips for people to listen to for themselves. I also did a separate shootout with a Studio Projects C3 which I'm going to include in a later post (so as to avoid confusion).
For those curious about my methodology, both mics were set up so as to capture the same performance simultaneously. In each test the mics were placed end to end. Both mics were tracked through a pair of Focusrite ISA One Preamps and into the aux in channels on my mBox 2 Pro.
I'd love to hear what folks think.
Here are clips from the shootout between the Studio Projects C3 and the Sennheiser MK4. The same methodology/gear used in the 414 shootout (above) was used to generate these clips.
Very cool of you to do this. I'll listen when back in my studio.
It was purchased very recently, so it's not one of the vintage ones I've heard people gush about (I have a friend with a 414 from the 70's that he swears by - I'll have to compare the two at some point). Anyone out there have a chance to AB a vintage 414 with a newer one?
I figured this would be useful to those interested in the MK4. I have my opinion about what I hear in these files, but I'd rather keep it to myself for the time being (so as not to color anyone else's take on what they hear).
Listening on Sony MDR-7506 on a laptop...they all sound pretty dang similar. With a gun to my head my pick here is the Studio Projects mic.
On the acoustic I prefer the sennheiser but they are both just ok imo (pretty different though).
On vocals it looses to both the akg and the studio projects, a bit too nasal (for this voice).
That was really awesome to hear. Thanks. You wouldn't happen to have a "blue bluebird" and/or an "AT4040" that you could shoot out with the mk4 would you? Thanks!
Can't say that I have either of those (although I understand why folks might find shootouts with those mics relevant/helpful). I chose the 414 because it is a respected, industry standard that many engineers are familiar with. I chose the SP C3 because it was the only cheap, Chinese LDC I had kicking around, and I thought that it would be useful for folks to hear how the MK4 would compare with that sound.
The guitar was a recently acquired Larrivee OM 03 (I love the way small bodied guitars record). The mics were placed end to end, pointing at the 14th fret from about a foot away from the guitar. Nothing fancy I think a lot of people mic a guitar using this general technique. By all means, try it out!
Agreed!!! And the Sennheiser sounds fantastic on it! Very rich and detailed...lots of sparkle. I prefer it over the 414 by a very wide margin in the guitar clips. Nice!
I prefer the 414 on both tracks over the Sennheiser. That surprises me because I have that model of 414 and always thought it sounded too bright. But the Sennheiser here is brighter than the 414. The Sennheiser here has some high end content that I find distracting and not adding anything to the sound. I listened on Sennheiser HD600 headphones.
Ric4001, I agree that the Sennheiser is bright (significantly brighter than the 414). I definitely prefer the 414 on the vocal. What surprised me is that I preferred the Studio Projects C3 to the Sennheiser on the vocal as well (I thought it had more presence). I really wasn't expecting the Sennheiser to sound "scooped" but that's how I would describe it. As for the guitar, I agree with Hossman777 that it captures the nice "sparkle" of this acoustic, and I can see how some might prefer the MK4. Of course much depends on how you want to use it in a mix. I could see using it for recording a rhythm acoustic track (I don't think I'd need to use a HPF on it). On the other hand, I don't think I'd want to use it to record a "lead" acoustic guitar (playing single note lines). For that I'd prefer the 414.
In the interest of being thorough, I thought I'd post two more sound files. This is a shootout between the MK 4 and the Studio Projects C3 on fingerpicked acoustic guitar. Again, I used the same methodology and gear that I used in the tests above.
Pretty interesting, wouldn't you say?
wow, my mk4 sounds rather different to me. interesting! probably my choice of mic placement - I always adjust a mic to sound it's best and when I do shootouts I don't keep the mic in the same place. which is why I don't do shootouts for anyone other than myself for my own comparisons.
each mic at it's best sounding position is what counts to me (I'm NOT saying that you didn't do that, but most people don't do that so you likely didn't do that either).
for me the mk4 sounds pretty amazing just a few inches from a voice, often 2 or 3 inches away. and while getting really close can make many mics sound better (not just proximity effect, intimacy and presence change dramatically as well), you still hear the sonic signature of the mic close up and I've gotten some amazing sounds on vocals this way over the years.
but overall this thread makes me unimpressed with the mk4.
quite different from another shootout I heard online a year or two ago where the mk4 really shines. wish I could remember the url, I know it wasn't on gearslutz.
I've had some good results using the MK4 up close as well. It gets sharp REALLY quick once you start backing off more than 6 inches. Still, I think I need to take a break from these threads. I started out loving this mic, but now I'm convinced I need to to sell it and get something more suitable for male vocals. How easily I'm swayed!
Follow your ears. If you like how it sounds and you've figured out a way to use it so as to get good results with it, then keep it around.
For this shootout I stayed as scientific as possible (same performance, same distances, identical preamps, etc...). Interesting that you were able to use the proximity effect on the MK4 to get better results. I don't like to HAVE to get too close to a mic while singing. Furthermore, I don't like to ask a client to get right up on the pop shield (that can be a little gross if you know what I mean). Also the increased possibility of bumping the mic and ruining the take starts become a bigger factor.
definitely - a mic that sounds incredible on lead vocals from 8" to 12" back is an incredible thing to have around.
However IMHO (just for my experience here...) it's not necessary at all to worry about having the singer up really close imho - most singers are used to eating mics on stage and think it's how it should be done. I've always had trouble forcing singers to stay back from a mic actually, even with a pop filter. Amazing when I think of how many times that I've had a singer push the pop filter stand closer (Either behind my back or just by pushing with thier faces against it). Maybe I need to bolt that thing down. I used to use it on the same stand but then you get noises when they push against it.
You make a good point. Not all mic proximity effects are created equal. You also had a good point earlier in the thread about comparing mics in a more subjective way (by finding each mic's optimal placement even if they differ). Of course if you used that approach for a shootout like this (and post it in a gear forum), the results will immediately be called into question. Nonetheless, the point is well taken. Thanks for the insight.
fully appreciate what you did in this thread. I agree, how else could you have done it without getting flamed? although I suppose the shootout you did followed by a similar redo but in what you felt were the most musical sounding positions for each specific mic - that might be the only way to please everybody.
but that's not just twice the work but more like 4 times the work thanks to all the mic experimenting involved, and no matter what, as you're likely thinking, people would be saying "why'd you put mic A 3 inches from the source? I always found if you turn it 20 degrees and keep it 1.7 inches from the source and put a pencil in front it's better than a C12!"


In the Central Reserve Police, applications for recruitment of 359 vacant posts of Constable and Head Constable under sports quota are invited. Interested candidates can apply before the final date by reading the given instructions.
The last date for application is January 13, 2019. Candidates for these positions will be selected on the basis of interview and experience.
Age limit – 18 -23 years. Please see the published notification for age relaxation and other information.
Educational Qualifications – 10 + 2 pass from a recognized board.
How to apply – Candidate for detailed notification and other information. Employment News paper 15 – 21 December 2018 Page No. 44 See.
Apply soon – 359 vacant posts of Constable and Head Constable under sports quota are invited. Interested candidates can apply before the final date by reading the given instructions.
For more information related to Central Reserve Police Force, you can see published notices. Please share this information with your friends and help them and visit daily on our website daily for employment.
Central Reserve Police Force (CRPF) is the main Central Police Force of the Union of India for internal security. It was originally constituted in 1939 as a Crown Representative Police, which is the oldest central semi-military force (now called the Central Armed Police Force).
The CRPF was developed in 1936 as a link to the agitations and political unrest in the then princely states of India, following the Madras Resolution of the All India Congress Committee, and to make it law and order in the form of royal policies.
To help the abundance of the vast majority of the indigenous states, the Crown representative was always developed for the ever increasing desire. Was there.


You certainly don't have to be Sheldon Cooper to enjoy the "temple of science". And you can see the stars in the sky even in bad weather. The projection of the artificial sky is extraordinary. If the weather is nice, though, you can see the night sky and have a great view on Brno as the planetarium is conveniently located in the area of Kraví hora – central and in a beautiful park.
Autosalon: International Motor Show. The soonest will be held 5.-8.4.2013 (the posters say 4.-8.4., but be careful, 4.4. is press day only, so you can't get in unless you are accredited).
Intercanis and Interfelis: International Dog and Cat shows (29.-30.6. 2013).
I don't want to bore you with all the fairs I'd love to go to, so check out the schedule for yourself, I'm sure you'll find something that you might be interested in. And you should go since the Trade Fairs compound, apart from the fair, is an interesting thing to see!
The Brno dam lake is a very popular place not only for tourists but for many locals as well. A bike trip round the lake is the best way of spending a Saturday! If you're too lazy to ride the bike, just take a walk or take a trip on the boat (the season is supposed to start on 11.4. 2013).
Take the boat to the Veveri Castle and spend some time there, too. The first reference to the castle is from the 13th century, today's look comes from the 14th. My secret tip: if you're not that much into castles, don't go for the inside tour, but the courtyards and tower are pretty amazing. The castle is currently undergoing a reconstruction, however, it will take a long time until it's finished. Take it as a rare opportunity to compare and contrast the reconstructed and original parts of the castle.
It is said that half of Brno goes to the dam lake and the other half to Marian Valley. And it is true. Marian Valley is easily reached by bus. The Marian Valley consists of "lakes" (man made water reservoirs that were built from 1953 to 1967) surrounded by forests. During your walk you can visit several mills, restaurants, playgrounds for children and three caves, two of which are freely accessible. Worth visiting!
This complex maze of underground tunnels and cellars opened to public in April 2011 after a large reconstruction and it is something that you absolutely have to visit. During a 45-minute tour you can discover the mysterious Brno underground with its dark corners and, on a brighter side, wine cellar. Some of the corridors date back to middle ages and they go as deep as 8 meters under the ground. How amazing is that?


"A consultant who knows how the regulator thinks" - "The Harmonised Offshore Chemical Notification Format (HOCNF) is the dataset and application format which is used to regulate the chemicals used by the Offshore exploration and production industry in the OSPAR sector of the North Sea. Having been the regulator for over 12 years during the formative phase of the HOCNF and having worked with the international group that developed the CHARM (Chemical Hazard and Risk Management) model there are few with Julia's experience available that can help make your submissions. Also if you need to reformulate to assist with the 'substitution' process, require justification for uses, need to run CHARM assessments or have any other queries relating to the HOCNF processes then Julia can help"
"A consultant who knows how the regulator thinks"
Copyright © 2011. Julia Osborne Consulting - All Rights Reserved.
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text:
Time Zone: Thomas County lies in the Central Time Zone (CST/CDT) and observes daylight saving time.
The community of Thedford is the Seat for Thomas County.
Thomas County was founded in 1887.
From the Census Estimates for 2009, <1> Thomas had a population of 565 people. This is a decrease of 22.5% since the last Census (which gave a population of 729 people in 2000).
At the time of the 2000 Census, Thomas represented 0.04% of the total population of Nebraska, making it the state's 89th most populous county (out of 93 counties).
The following table shows the recent changes in population. Other than 2000, the population counts have been estimated by the Census Bureau.
Year Population Change
Since 2000 Year-to-Year Change
2010 647 -11.25% +14.51% since 2009
2009 565 -22.5% -3.09% since 2008
2008 583 -20.03% -2.83% since 2007
2007 600 -17.7%
2000 729 The Last Census
More information can be found on the Thomas County Census Page for Thomas County.
Communities in Nebraska
<1> On a yearly basis, the US Census Bureau creates an estimate of the county's population. Keep in mind that this is an estimate and not an actual count. The last physical count was the 2000 Census and the next count will be for the 2010 Census.
<2> All Quarter-dollar coin images from the United States Mint.


text:
Always Improving
The 2023 model year is starting. Is your company up-to-date on the newest industry standards?
NMMA and ABYC, through certification and standards, work hard to ensure the end user is safe on the water.
Courtesy NMMA; GARY REICH
We are in the middle of peak boating season, a busy time for the recreational boating community, marine manufacturers and certification teams. While we're seeing sales begin to stabilize following historic growth in 2020 and 2021, new-boat sales remain above prepandemic levels. For the second time in 15 years, first-time boat buyers exceeded 415,000, accounting for 34 percent of boat sales in 2021, driving growth for the boating industry and further reinforcing heightened demand for boats since the outset of the pandemic.
As the 2023 model year begins, it's important to stay up-to-date with changes to industry standards. The American Boat and Yacht Council published the Standards and Technical Information Reports for Small Craft, Supplement 62, in late July. Included in this supplement are more than 15 standards updates, along with three new standards.
Of the three new standards, the ABYC E-30, Electric Propulsion Systems, was recently adopted into the NMMA Certification program. This standard addresses the design, construction and installation of alternating current and direct current electrical systems on boats for the purpose of propulsion.
The E-30 standard covers topics such as labeling and warnings, monitoring, grounding, battery switches and more. If you are building or plan to develop boats with electric propulsion systems, this standard is an excellent resource.
Updated standards include E-13, Lithium-Ion Batteries; S-32, Warnings and Safety Signs for Boats; T-33, Manufacturers Statement of Origin; A-32, AC Power Conversion Equipment and Systems; H-8, Buoyancy in the Event of Flooding/Swamping; H-24, Gasoline Fuel Systems; H-29, Canoes and Kayaks; H-30, Hydraulic Systems; H-35, Powering and Load Capacity of Pontoon Boats; H-37, Jet Boats - Light Weight; H-41, Reboarding Means, Ladders, Handholds, Rails and Lifelines; P-21, Manual Hydraulic Steering Systems; P-23, Mechanical Steering and Propulsion Controls for Jet Boats; S-30, Outboard Engine and Related Equipment Weights; S-31, Environmental Considerations for Systems and Components Installed Onboard Boats; T-1, Aluminum Applications for Boats and Yachts; TE-12, Three Phase AC Electrical Systems on Boats; TH-12, Outboard Engine Mounting Guide; TH-22, Educational Information about Carbon Monoxide; and TH-23, Design, Construction and Testing of Boats in Consideration of Carbon Monoxide.
We would like to remind builders of six things to keep in mind during model-year transition. With ongoing supply-chain challenges, it's imperative for engineering and compliance teams to work with sourcing groups and ensure all components are designed for and approved for use in a marine environment.
The design group plays a decisive role in the new components and parts for the product line. The supply chain should include every possible component part switched over for the 2023 model year. Sales and marketing must effectively communicate and promote any product updates, from digital to brochures to e-mail. Logistics teams should ensure that everyone in the facility and warehouse have what they need, and that it is accounted for on the production floor. Production teams need to be aware of all new installations or changes that new components and accessories may bring.
And, last, NMMA Certified inspectors should be part of the process. Annual inspection schedules are filling up fast. Reach out to an NMMA inspector today to be inspected as early in the model year as possible, to mitigate potential exposure.
NMMA Certification is the premier product certification program for boats, yachts, boat trailers, personal watercraft and marine oils in the United States. It's our mission to help marine manufacturers succeed in providing safe products for the boating industry. Many — but not all — boats are required to meet a set of minimum manufacturing regulations established by the Coast Guard. In the United States, NMMA Certification goes beyond Coast Guard standards to ensure adherence to ABYC standards. Manufacturers of NMMA Certified boats receive a detailed inspection and verification process; improved consumer confidence; increased brand respect; and liability protection and product liability insurance discounts.
For more information on NMMA Certification, visit nmma.org/certification.
Scott Berry is senior director of engineering standards for the National Marine Manufacturers Association.
American Boat and Yacht CouncilWater SafetyNMMA CertificationIndustry StandardscertificationBoating


text:
\section{Introduction}

M15 is renowned for containing the first globular cluster
Low-Mass X-ray Binary (LMXB; X2127+119) to be
optically identified (with AC211, see Auri\`ere, Le Fevre \& Terzan
1984 and Charles, Jones \& Naylor 1986), a counterpart that is still
one of the most optically luminous of all LMXBs.
AC211 is also the first globular cluster X-ray source
to have both an optical and X-ray
demonstration of its 17.1 hour orbital period via extended, partial
eclipses (see Ilovaisky et al. 1993 and
Ioannou et al. 2002 and references therein).  Subsequent
studies of M15 show that it contains additional exotic, highly evolved
binaries. For example, there are at least 8 millisecond pulsars (MSP),
6 of them within 8 arcsec of the cluster core (Kulkarni \& Anderson
1996). Two of these MSPs have a negative $\dot{\rm P}$ (i.e. an
acceleration toward us as they move in the cluster potential) implying
a mass concentration of $\sim$ 4000
${\rm M}_{\odot}$ at the cluster centre (Phinney 1996). Phinney argues
that this mass {\it cannot} consist of low-mass stars and is either a
central black hole, or more likely a concentration of stellar
remnants: neutron stars and white dwarfs.

M15 is one of the most metal-poor globular clusters known ([Fe/H]
$\sim -$2.1) and has a low reddening factor (E$_{B-V} = 0.10 \pm
0.01$; Harris 1996).
A recent study has refined the distance to M15 to 9.98$\pm$0.47~kpc
(McNamara, Harrison \& Baumgardt 2004) which places it 5\% closer than
the previously quoted value of 10.4$\pm$0.8~kpc (Durrell \& Harris
1993).
McNamara et al. (2004) also provide a new estimate for the age and the
mass of the cluster which are 13.2$\pm$1.5~Gyr and (4.5$\pm$0.5)$\times
10^5$~${\rm M}_{\odot}$\, respectively.
M15's main-sequence turn-off point lies at $V \simeq 19.4, B-V \simeq 0.47$.

M15 was for a long time believed to be a classic example of a
central-surface-brightness-cusp globular cluster (Newell \& O'Neill
1978; Djorgovski \& King 1986; Peterson, Seitzer \& Cudworth 1989),
i.e. a cluster which has undergone core-collapse, with a small ($\sim$
0.06 pc), densely-crowded core containing many non-luminous remnants,
or even a single, massive black hole. However, more recent work shows
that M15's core, while compact, is larger than previously thought
(0.13 pc; Lauer et al. 1991), and the central velocity dispersion
lower ($\sim$ 10 km~s$^{-1}$; Gebhardt et al. 1992). As a result, it
is no longer possible to tell whether M15 has, in fact, undergone
core-collapse: a classical pre-collapse, thermal equilibrium cluster
model fits the data just as well as post-collapse models with a
re-expanding core (Grabhorn et al. 1992; De Marchi \& Paresce 1994).

Recently, van der Marel et al. (2002) and Gerssen et al. (2002, 2003),
using longslit spectra obtained with the Hubble Space Telescope (HST), have
shown that radial velocity measurements are consistent with a central
dark mass.  Models of the data which include a central black hole of
mass $\sim 2000$~${\rm M}_{\odot}$\, fit the data slightly better than models
without one. However, a central concentration of non-luminous, massive
stellar remnants fits the data just as well, as shown in the dynamical
simulations of Baumgardt et al. (2003).  Furthermore, the {\it Chandra}
X-ray images presented by White \& Angelini (2001) show no evidence
for any X-ray emission at the cluster centre, again indicating that it
is unlikely to harbour a central black hole (see also Ho, Terashima \&
Okajima 2003).

One of the primary motivations for this project was to attempt to
solve one of X2127+119/AC211's biggest mysteries: the X-ray
and optical light curves, and its very low $L_{X}$/$L_{opt}$, show unambiguously
that it is an accretion disc corona source (e.g. Ilovaisky et
al. 1993; Ioannou et al. 2002), in which the compact object is
obscured at all times by the accretion disc. But luminous type I X-ray
bursts have been observed from the system (e.g. Dotani et al. 1990),
requiring that a neutron star is visible (at least at certain times)!
We inferred therefore that X2127+119 may actually consist of {\it two}
luminous X-ray binaries in M15's core, too close together to be
resolved by previous X-ray observations (Charles, Clarkson \& van Zyl
2002). This suggested exploiting {\it Chandra's} superb
$\sim$0.5-arcsec spatial resolution, and the result was the High
Resolution Camera (HRC-I) images presented here, in order to search
for additional sources close to AC211.

However, before the HRC-I observations were performed, White \&
Angelini (2001) serendipitously resolved X2127+119 into two bright
LMXBs with the zero-order ACIS-S/HETG image. M15~X-2 was found to be
associated with a $U\sim19$ star located 2.7 arcsec from AC211 and 3.3
arcsec NW of the cluster core. While M15~X-2 is $\sim$4 mag fainter
than AC211, it has an X-ray count rate $\sim$2.5 times
greater. Nothing is known yet about the nature of M15~X-2, other than
that -- if we assume it to be responsible for the type I X-ray bursts
(and thereby resolving the controversy of AC211's X-ray properties) --
the compact object is a neutron star. This then leaves the nature of
the object in AC211 unconstrained.

High resolution X-ray imaging is now revealing a wide range
of low-luminosity sources in globular clusters (see e.g. Heinke et
al. 2003a; Hakala et al. 1997).
The advent of {\it Chandra} has made it possible to investigate these sources
in earnest. Some of the first results, (e.g. Pooley et al. 2002a,b),
show detections of CVs in the globular clusters NGC~6752 and
NGC~6440. Dozens of low-luminosity X-ray sources have also been
discovered in $\omega$ Cen and NGC~6397 (see Verbunt \& Lewin 2004
for a recent review), and $\sim$300 in 47 Tuc (Heinke et al. 2004).

These studies are narrowing the gap
between the predicted and observed CV population densities, but have
been primarily restricted to the cases of those clusters that do {\it
  not} contain central luminous steady LMXBs.
However, one should note that a number of studies has emerged recently using
 {\it Chandra} to look for faint sources in globular clusters which do
 contain bright LMXBs, e.g. Heinke, Edmonds \& Grindlay (2001), Heinke
 et al. (2003b), Wijnands et al. (2002), Homer et al. (2002).

M15 is a good cluster to hunt for CVs and LMXBs because of its
large mass and high compactness: its very dense core should be an
ideal breeding ground for CVs and LMXBs (as indicated already by the
MSP population).
In addition, its very low reddening will not hinder the UV/optical
identification of any new sources that are found.

What are the chances of optically detecting a dwarf nova (DN)
in outburst in M15 during a single HST visit? Di Stefano \& Rappaport (1994)
predicted a population of $\sim$ 200 CVs in 47 Tuc, of which $\sim$ 50
are DNe. We would expect M15 to have a much higher population of CVs
because of its greater core mass and central condensation than 47 Tuc.
Nevertheless, assuming that M15 has say 50 DNe, with a mean outburst
recurrence time of 50 days and outburst length of 10 days, then at any
given time, one would expect to see $\sim$10 DNe in outburst.

Although DNe are brighter in the optical during outburst than
in quiescence, their behaviour in the X-ray is harder to predict.
A good summary of the current view of the origin of the X-rays is
given by Verbunt, Wheatley \& Mattei (1999).
For our purposes the crucial point is that in outburst the 2.5--10~keV
flux from the boundary layer largely disappears, and is replaced by a
very soft extreme ultraviolet (EUV) component.
The disappearance of the hard component should drive the X-ray flux
down in outburst, but the EUV component is so luminous that if its
hard energy tail reaches the soft X-ray range, it will dominate the
flux there, and lead to a brightening in that range.
Thus whether the DN brightens or fades depends crucially on the
X-ray energy range in question, and to a lesser extent the reddening.
Given that we know at least one DN (U Gem; Swank et al. 1978) whose
flux increases even in the 2--10~keV range, some DNe will be brighter in
outburst than quiescence in HRC-I, but it is not clear this is true for
all of them.

From an observational point of view, we are particularly interested in
the DNe subclass of CVs because of their frequent outbursts making
them easier to detect and classify as definite CVs. Outburst
recurrence intervals for DNe range typically from 14 -- 120 days or
longer, and last $\sim$10 days (see e.g. Warner 1995).

Hence, we use our {\it Chandra} data here to investigate these fainter
sources, in an attempt to reveal M15's menagerie of CVs, quiescent
low-mass X-ray binaries, (chromospherically) active binaries
and other exotica for the
first time. This work is still in progress: detecting the faint X-ray
sources in the core, which is dominated by the flux from AC211 and
M15~X-2, has been -- and continues to be -- a considerable challenge as we
will discuss below.

In Section~\ref{chandra} we present our {\it Chandra} HRC-I observations,
with particular emphasis on how to remove the two luminous sources so
as to reveal the faint population within. In Section 3, we
use archival HST imaging to search for optical counterparts to these
faint X-ray sources and discuss the implications of these results for
the nature of this faint source population.

\section{{\it Chandra} HRC Imaging}\label{chandra}

\subsection{Observations}

We obtained three separate observations of M15 with {\it Chandra's}
  HRC-I (Murray et al. 1997) of approximately 10~ksec each over a six
  week period in 2001~Jul--Aug.
The HRC-I has a $30^{\prime}\times30^{\prime}$ field of view.
Table~\ref{tab-obs} summarizes the details of the observations.
All data were reduced and analyzed using {\sc CIAO} versions 2.0 to 2.3.

Figure~\ref{fig-m15} shows our summed HRC-I image of the central region
  of M15.
The crosses show the positions of 7 of the 8 known MSP's, while
  the circle represents the $2^{\prime\prime}.2$ core radius centred on
  the position of the cluster centre ($\alpha=21^h29^m58.^s335,
  \delta=12^{\circ}10^{\prime}0.^{\prime\prime}89$, J2000; van der Marel
  et al. 2002).
The {\it Chandra} and HST images (Sec. 3) were realigned on the basis of the
  AC211 positional match.

\begin{table}
\caption{{\it Chandra} observation log}
\label{tab-obs}
\begin{tabular}{cccc}
Observation number & Date        & UT$_{\rm start}$    & UT$_{\rm stop}$ \\\hline
1903               & 2001 Jul 13 & 07:07:43           & 10:04:42 \\
2412               & 2001 Aug 3  & 16:24:35           & 19:23:48 \\
2413               & 2001 Aug 22 & 04:57:07           & 08:23:19 \\ \hline
\end{tabular}
\end{table}

\begin{figure}
\includegraphics[width=80mm]{ME1057_figure1.ps}
\caption{Our summed HRC-I image of the centre of M15, showing the two
 bright sources, AC211 and M15~X-2, and the positions of 7 of the
8 known millisecond pulsars (from {\sc SIMBAD}). The circle represents the
 location and extent of the cluster core (which has a radius of 2.2
 arcsecs, see Lauer et al. 1991).  }
\label{fig-m15}
\end{figure}

Figure~\ref{fig-lc} shows the light curves obtained for AC211 and M15
  X-2 during the three observations.
The phase of each observation,
  obtained using the ephemeris in Ioannou et al. (2002),
  is given in each plot.
They show that the
  observations were undertaken just prior to the eclipse in AC211.
It is clearly seen that M15~X-2 is a steady source with an average count
  rate of 6.8 ct/s, while AC211 enters a flaring state during the last
  observation on 2001 Aug 22.

Table~\ref{tab-fl} shows the average count rates and the fluxes
  derived for both sources using the spectral parameters from White \&
  Angelini (2001).
For M15~X-2 we fixed the hydrogen column density to the expected value
  of M15, i.e. $N_H=6.7\times10^{20}$~cm$^{-2}$, and used a power law
  with an index of 1.89 to derive the 0.5--7.0~keV luminosity.
In the case of AC211, we used the partial covering model
  with a power law photon
  index of 2.0, a covering fraction of 0.92 and an intrinsic
  absorption of $2.05\times10^{22}\,{\rm cm}^{-2}$.
Again, the interstellar absorption was set to that of M15.
Assuming a distance of 9.98~kpc to M15, these
  convert to an average luminosity of $L_x=1.4\times10^{36}~{\rm
  erg}~{\rm s}^{-1}$ for M15~X-2 (consistent with that found by White \&
  Angelini, although note that they used the previous value for the
  distance to the cluster of 10.3~kpc)
  while AC211 varies between $L_x=7.9\times10^{35}~{\rm
  erg}~{\rm s}^{-1}$ in the first observation to
  $L_x=2.2\times10^{36}~{\rm erg}~{\rm s}^{-1}$ in the last observation.

The luminosity of M15~X-2 is consistent with that of White \& Angelini
(2001), as are the luminosities for AC211 in observations 1903 and
2412. However, the luminosity of AC211 in observation 2413 is significantly
higher than in the other two observations, and indicates a brightening
of the source at that time.

Table~\ref{tab-fl} also shows the count rate and X-ray luminosities
for source D, most likely identified with the planetary nebula (PN)
K648, as we discuss in more detail in Section~2.2.

\begin{figure*}
\includegraphics[width=160mm]{ME1057_figure2.ps}
\caption{The light curves of AC211(top) and M15~X-2 (bottom) from the
  three observation dates. The binary phase of AC211 is given on the
  plots at the beginning and end times.
}
\label{fig-lc}
\end{figure*}

\begin{table*}
\caption{Count rates and luminosities}
\label{tab-fl}
\begin{center}
\begin{tabular}{ccccccc}\hline
Obs. no.  & \multicolumn{2}{c}{1903} & \multicolumn{2}{c}{2412} & \multicolumn{2}{c}{2413} \\\hline
  & Count rate  & L$_{\rm X}$ (0.5--7 keV)  & Count rate  &  L$_{\rm X}$ (0.5--7 keV)  & Count rate  & L$_{\rm X}$ (0.5--7 keV)  \\
  & (s$^{-1}$)  & (erg s$^{-1}$) & (s$^{-1}$)&  (erg s$^{-1}$) &(s$^{-1}$) & (erg s$^{-1}$) \\\hline\hline
AC211    & 1.55$\pm$0.18 & $7.9\times10^{35}$ & 1.65$\pm$0.19 & $8.4\times10^{35}$ & 3.87$\pm$0.27 & $2.2\times10^{36}$ \\
M15~X-2  & 6.97$\pm0.36$ & $1.4\times10^{36}$ & 6.57$\pm0.35$ & $1.3\times10^{36}$ & 6.95$\pm0.36$ & $1.5\times10^{36}$ \\
K648  & $0.26\pm0.18\times10^{-3}$ & $2.6-6.1\times10^{31}$$^{\star}$
  &$<0.06\times10^{-3}$ & $<0.6-1.4\times10^{31}$$^{\star}$ & $1.03\pm0.42\times10^{-3}$
  &$1.0-2.4\times10^{32}$$^{\star}$ \\ \hline \hline
\end{tabular}
\end{center}
\hspace{-140mm}{\footnotesize $^{\star}$ See Table~\ref{tab-xraysources} and Section 2.2.}
\end{table*}

\subsection{Searching for faint sources}

The main problem in detecting faint sources in M15 is that, unlike
for instance the
clusters studied by Pooley et al. (2002a,b) in which there are no
X-ray bright sources, M15 houses not just one but {\em two}
bright central sources. Any faint sources lurking near the centre of
the cluster -- which is where we would expect to find them -- will be
contaminated by the wings of the AC211 and M15~X-2 point spread functions
(PSF).  Thus to have any hope of detecting faint sources, the two
bright central sources must first be subtracted. We did
this by constructing a PSF for each of the two sources using the {\it
Chandra} PSF libraries. To increase the signal-to-noise of any
possible faint sources, we merged the three observations.  We then
used the faint source algorithm {\sc wavdetect} on the PSF-subtracted
merged image.

Figure~\ref{fig-psf} shows both the merged image (a) and the resulting
PSF-subtracted image (b) of
the merged observations. They both show the positions of
potential sources (A and B) found after {\sc wavdetect} was run on the
PSF-subtracted image. As can be seen immediately from these images,
the software and understanding of the {\it Chandra} PSF is not yet
able to smoothly subtract bright sources from images without leaving
large-scale (but smooth) artefacts such as the central ``hole''.
Nevertheless, it
does allow a more sensitive search for fainter sources to be
undertaken on the subtracted image, and we can gauge the effectiveness
of this analysis to search for potential counterparts
by using archival Hubble Space Telescope images. In
addition to the sources found close to AC211 and M15~X-2, {\sc wavdetect} also
found two sources (C and D) at larger radii, one being the planetary
nebula K648, shown in Figure~\ref{fig-dn+pn}.

Table~\ref{tab-sources} shows the coordinates and {\it U}-magnitudes
for the four sources found in and near the centre of M15.
Table~\ref{tab-xraysources} shows the X-ray luminosities
for these four sources estimated using typical spectral parameters,
based on our candidate IDs.
For sources A and C (DNe) we used a Bremsstrahlung
  temperature of 4~keV.
The merged dataset was used to extract the
  parameters for source A.
For source B (qSXT/DN?) we applied several models.
We used the parameters for Aql X-1 in {\it quiescence}
(taken from Rutledge et al. 2001 using {\it Chandra} data).
Two estimates were derived, one for a power law with photon
  index 4.1 and one for a blackbody temperature of 0.33~keV.
In addition, we also used a Bremsstrahlung temperature of 4~keV.
Finally, for source D (PN) we applied two models: we used
  parameters from Guerrero et al. (2001), i.e. a Raymond-Smith model with
  temperature 0.64~keV, and -- in the case that the emission might
  arise from a compact region (as discussed in Section~3.3) -- we
  applied a thermal Bremsstrahlung temperature of 4~keV.
We discuss the nature of these sources
  and compare them to HST data in the next section.

\begin{table*}
\caption{Optical counterparts of faint {\it Chandra} sources in M15}
\label{tab-sources}
\begin{center}
\begin{tabular}{cccccc} \hline
ID & Object&   Location$^{\star}$ &  Coordinates (J2000) &  {\it U}-magnitude &  Variable? \\
   &    &          &               RA DEC   & & \\ \hline
A & DN    & 0.3'' NE & $21^h29^m58.37^s +12^{\circ}10^{\prime}00.8^{\prime\prime}$ & 17.6$^{\dagger}$ & Yes \\
B & qSXT/DN? & 11.'' N  & $21^h29^m58.32^s +12^{\circ}10^{\prime}12.4^{\prime\prime}$ &  21.8 & Possibly \\
C & DN    & 46.'' NE & $21^h29^m57.34^s +12^{\circ}10^{\prime}43.7^{\prime\prime}$ &  20.2$^{\dagger}$ & Yes \\
D & K648  & 31.'' NW & $21^h29^m59.38^s +12^{\circ}10^{\prime}27.5^{\prime\prime}$ & 13.5$^{\ddagger}$ &Yes (X-rays) \\\hline \hline
\end{tabular}
\end{center}
\hspace{-70mm}{\footnotesize $^{\star}$With respect to the cluster centre.}\\
\hspace{-40mm}{\footnotesize $^{\dagger}$Magnitude in outburst (object not visible in quiescence).}\\
\hspace{-70mm}{\footnotesize $^{\ddagger}$from Alves, Bond \& Livio (2000).}
\end{table*}

\begin{figure}
\includegraphics[width=80mm]{ME1057_figure3.ps}
\caption{{\bf (a)} The merged image of all three observations
  of the centre of M15, showing the two bright LMXBs.
{\bf (b)} The image after PSF-subtraction of these sources;
the two faint sources detected by the source detection algorithm
{\sc wavdetect} in this image are overlaid in both panels.}
\label{fig-psf}
\end{figure}

\begin{figure}
\includegraphics[width=80mm]{ME1057_figure4.ps}
\caption{{\it Chandra} HRC-I image showing the locations of a
possible dwarf nova (source C) and the planetary nebula, K648 (source D),
detected using {\sc wavdetect}, both well within the half-mass radius.
The image is approximately 90$^{\prime\prime}$ (width) by
70$^{\prime\prime}$ (height). The bar shows 5$^{\prime\prime}$.
}
\label{fig-dn+pn}
\end{figure}

\begin{table*}
\caption{X-ray luminosities of faint {\it Chandra} sources in M15
  assuming a distance of 9.98~kpc}
\label{tab-xraysources}
\begin{center}
\begin{tabular}{cccccc} \hline
   \multicolumn{6}{c}{X-ray luminosities (erg s$^{-1}$ in the
   0.5--7~keV range)} \\ \hline
   & & & \multicolumn{3}{c}{Obs \#} \\
Source  &       &   Model  &                 1903   &   2412   & 2413 \\ \hline \hline
 A      &  DN   & kT$_{\rm Bremss}$=4 keV &         & $3.3\times10^{32}$$^{\dagger}$ & \\
 B      & qSXT? & $\alpha=4.1$  & $2.34\times10^{31}$ & $7.30\times10^{31}$ & $1.15\times10^{32}$ \\
        &       & kT$_{\rm BB}$=0.33 keV & $4.28\times10^{31}$ & $1.34\times10^{32}$ & $2.10\times10^{32}$ \\
        &  DN?  & kT$_{\rm Bremss}$=4 keV & $7.46\times10^{31}$ & $2.33\times10^{32}$ & $3.66\times10^{32}$ \\
 C      &  DN   & kT$_{\rm Bremss}$=4 keV & $8.65\times10^{31}$ & $1.94\times10^{32}$ & $1.66\times10^{32}$ \\
 D      & K648  & kT$_{\rm RS}$=0.64 keV & $2.6\times10^{31}$ & $<0.6\times10^{31}$ &
   $1.0\times10^{32}$ \\
        &       & kT$_{\rm Bremss}$=4 keV & $6.1\times10^{31}$ &
   $<1.4\times10^{31}$ & $2.4\times10^{32}$ \\ \hline
\end{tabular}
\end{center}
\hspace{-70mm}{\footnotesize $^{\dagger}$ The merged dataset was used
  to derive the luminosity of source A.}
\end{table*}

To estimate whether any of the four faint sources may actually be
  background sources, we use the log N -- log S relations of Giacconi et al.
  (2001).
Using the count rate of our faintest source to set a flux
  detection limit (and assuming that it is in fact a typical
  background object with $\Gamma=1.5$), we obtain
  $F_{lim} \simeq 2$ (0.5-2 keV) and 4.5 (2-10 keV) $\times10^{-15}
  {\rm erg}~{\rm s}^{-1}~{\rm cm}^{-2}$,
  and hence we expect $\simeq 0.5$ discrete background
  sources within the area enclosed by the half-mass radius
  (1.06$^{\prime}$) of M15.
This provides an upper limit since, even with our PSF subtraction,
  much of the central region of M15 is not probed
  to this depth.
We conclude that at most one source could be a background
  object, but given our optical counterpart IDs (see next section) we would
  suggest that they are all in fact associated with M15.

\section{HST Imaging and the Nature of the Low $L_X$ Sources}

M15 has been a regular target for HST. Studies of M15's stellar
population have been carried out, for example, by Ferraro \& Paresce
(1993), De Marchi \& Paresce (1994; 1996) Guhathakurta et al. (1996)
and Sosin \& King (1997), and an intensive photometric study of M15's
PN, K648, was undertaken by Bianchi et al. (1995; 2001) and Alves,
Bond \& Livio (2000). The HST archives therefore contain many images
of M15 obtained at different epochs.

At the distance to M15, DNe would be expected to
have quiescent apparent magnitudes of 21 to 24, with outburst
magnitudes ranging from 14 to 21. Magnetic CVs would have magnitudes
similar to quiescent DNe (see Warner 1995), while the high mass
transfer rate CVs (the nova-likes and nova remnants) would be 2--3
magnitudes brighter. X-ray transients would be expected to have
quiescent apparent magnitudes similar to those of DNe, and outburst
magnitudes ranging from 13 to 18. The deepest HST archival images of
M15 go down to 22--23 mag. Therefore, most quiescent CVs and X-ray
transients would be too faint to detect in such images.

\subsection{Probable Dwarf Novae}

We looked for variables in M15's core by aligning and subtracting
images from different epochs, a technique which highlights stars which
vary between the images. In addition to detecting two
previously-identified RR Lyrae stars (Ferraro \& Paresce 1993), we
made a first detection of a probable DN in outburst
(Fig.~\ref{fig-DNs}a), located just 0.3 arcsec from the cluster core
(the optical discovery was reported in Charles, Clarkson \& van Zyl
2002). The object appears in WFPC2 {\it U}-band images taken in October 1994
with  {\it U}=17.60, but is undetectable in images obtained at
other epochs. Therefore its variability range is $>$5 magnitudes (the
deepest available images have a limiting {\it U}$\sim$22.5). This object is
revealed here to coincide with one of our
faint {\it Chandra} X-ray sources (source A); its luminosity of
$3.3 \times 10^{32}$~erg~s$^{-1}$ is consistent with the brighter CVs
identified in other globular clusters.
Outbursting DNe often start off hard, but this quickly disappears to
be replaced by a much softer component (see e.g. the light curves
of SS Cyg in outburst in Kuulkers et al. 2003).
However, we have no way of knowing
at what stage in its activity cycle it has been observed.

\begin{figure}
\includegraphics[width=80mm,angle=0]{ME1057_figure5.ps}
\caption{(a) Probable dwarf nova (source A) in the core of M15, found
using image-subtraction, reported in Charles, Clarkson \&
van Zyl (2002), found here to be associated with a {\it Chandra}
X-ray source. (b) Probable dwarf nova (source C) associated with a
{\it Chandra} X-ray source, located $46^{\prime\prime}$ NE of
the cluster core. The error circles are the {\it Chandra}
0.25~arcsec error circle.
}
\label{fig-DNs}
\end{figure}

If this object is indeed a DN or an X-ray transient, it is
statistically much more likely to be the former than the latter. DNe
outburst recurrence times are weeks to months, while X-ray transients
usually recur on much longer timescales, typically tens of years. The
chances of catching an X-ray transient in outburst on the few
occasions on which the HST has observed M15 over the last decade are
therefore extremely small.  The likelihood that we have a DN rather
than an X-ray transient depends also on the relative numbers of these
two kinds of object in the core of M15:
we expect CVs to be more numerous than X-ray binaries.
However, we do note that the (neutron star) transients in globular
clusters appear to have shorter recurrence times between outbursts
than those in the field (e.g. NGC~6440, Pooley et al. 2002b).
With all of those in clusters having been
identified as neutron star systems (due to the presence of type I
X-ray bursts), they represent a different population from the soft
X-ray transients overall, of which only $\sim$25\% contain neutron
stars, the rest being black-hole candidates (see e.g. Charles 2001).
And since the well-known neutron star SXT Aql X-1 outbursts once or
twice per year (e.g. Simon 2002),
it is still possible that our source A might not
turn out to be a DN.

The second probable DN was found in the error circle of a faint
{\it Chandra} X-ray source 46 arcsec NE of the cluster core (source C in
Figure~\ref{fig-dn+pn}, well within the cluster half-mass radius). It
appears in outburst with {\it U}=20.24 in images obtained in October 1994
(Fig.~5b), but is completely absent in images at other epochs. Again,
as we have no constraint on the light curve there is no
way of telling whether we caught it at the peak of its outburst, but
this magnitude is consistent with the DN outburst range (14 to 21)
expected for M15. Of course, it is also possible that this object is
an X-ray transient, but using the same arguments as above, we
believe it is more likely to be a DN.

Tuairisg et al. (2003) conducted a ground-based search in 1997 for
outbursting DNe in M15 but failed to find any.
If these sources (A and C) do turn out to be outbursting DNe, then
these are amongst the few identified thus far in globular
clusters -- only a handful of erupting dwarf novae in globular
clusters have been confirmed (or suggested as possible outbursting DNe)
to date (e.g. M22, Anderson, Cool \& King 2003; M5, Kaluzny et al. 1999;
47~Tuc, Edmonds et al. 2003).

\subsection{Possible qSXT or DN?}

 \begin{figure}
\includegraphics[width=80mm,angle=0]{ME1057_figure6.ps}
\caption{Possible qSXT? The faint blue star indicated appears to be
  variable. The error circle is the {\it Chandra} 0.25
  arcsec error circle.
}
\label{fig-maybeqSXT}
\end{figure}

The two sources discussed above are designated `probable' DNe, because
 they were obviously variable in the HST images and showed possible
 outbursts. The object discussed in this section is harder to
 classify, but is the only blue star near the corresponding
 {\it Chandra} X-ray source (Fig.~\ref{fig-maybeqSXT}).
The source in question is source B in Fig.~\ref{fig-psf}
and the possible counterpart is listed in Table~3.
 As explained in Section~2.2, we calculated its X-ray luminosity based on
 several models -- two for a possible qSXT scenario and one for a
 possible DN scenario (see Table~4).

In all three cases, the X-ray source has a luminosity of a few
$\times10^{31}$ -- $10^{32}$~erg~s$^{-1}$.
The candidate optical counterpart has {\it U}=21.8, {\it V}=22.54,
and appears to show some variability ($\Delta V\sim0.04$),
although this is uncertain -- the object is extremely
faint and the apparent variability may simply be noise
(van Zyl 2002).
Its X-ray luminosity is more consistent with that of a CV, although
it is also comparable to the faint end of the distribution of
qSXTs in GCs (Heinke et al. 2003a).
With $U-V=-0.74$, its optical colours  are again consistent with
those of the DNe SS Cyg and VW
Hyi in quiescence (Bailey 1980), similar to that of the NS SXT Cen X-4
in quiescence (McClintock \& Remillard 2000), but much bluer
than the optically identified qSXT (X5) in 47 Tuc (Edmonds et al. 2002).
We therefore suggest that source B is more likely another CV
rather than a qSXT.

\subsection{The Planetary Nebula K648}

The fourth faint X-ray source we detected has a position consistent
  (within the {\it Chandra} uncertainties) with one of the rare globular cluster PNe,
  K648  (Alves, Bond \& Livio 2000; hereafter ABL).
The source was seen to vary by a factor greater than three
  during the {\it Chandra} observations, being observed at
  $L_X=0.26$ and $1.0\times10^{32}$erg~s$^{-1}$ in two (\#1903,
  \#2413) but undetected in the third (\#2412).
We can reject that the source is constant at the $>$98\% level.
However, its luminosities are within the range 3$\times$10$^{29}$
  to 3$\times$10$^{32}$ erg~s$^{-1}$ in the
  0.4--1.7~keV band found for 13 X-ray-active PNe in the galactic
  plane using the ROSAT archive by Guerrero, Chu \& Gruendl (2000),
  and for the well-resolved, extended X-ray emission detected with
  {\it Chandra} from the PNe BD+30\deg3639 (Kastner et al. 2000) and
  NGC~7027 (Kastner, Vrtilek \& Soker 2001).
Presuming, therefore, that K648 is the source of the X-rays, it
  would be both the first globular cluster and the most distant
  X-ray detected PN.

Only four globular cluster PNe are known (see ABL and references
  therein), but their very existence implies an unusual
  evolutionary path.
The lower the mass of a post-asymptotic giant branch (AGB)
  remnant, the longer it takes to heat
  up to temperatures sufficiently hot to ionize
  the ejected envelope and produce a visible PN, by which time the
  ejecta may have dissipated.
Recent HST studies of white dwarfs in globular clusters indicate that
  AGB remnant masses are very low ($0.50
  \pm 0.02$ ${\rm M}_{\odot}$; Renzini et al. 1996; Cool, Piotto \& King 1996;
  Richer et al. 1997).
AGB remnants with these masses have evolutionary
  timescales that are much longer than PNe dissipation timescales
  (Sch\"{o}nberner 1983; Vassiliadis \& Wood 1994).
Therefore, we should not expect to observe {\it any} PNe within
  globular clusters!
Jacoby et al. (1997) have suggested that the globular cluster PNe were
  therefore formed through close binary interactions.

This certainly applies to the case of K648 since the most massive
  main sequence stars in M15 should have masses $M \leq 0.8$~${\rm M}_{\odot}$,
  with AGB remnant masses too low to
  produce PNe.
Moreover, ABL measured an anomalously high
  mass of $0.60 \pm 0.02$~${\rm M}_{\odot}$\space for the central
  star of K648.
They suggest the most likely origin for this higher mass white
  dwarf is from mass augmentation of its progenitor star (i.e.
  formation of  a blue straggler) due to either mass transfer in or
  merger of a close binary.
They also note that the morphology of K648 is typical of elliptical
  PNe.
This could be accounted for by either nebular ejection during a common
  envelope phase, or by enhanced rotation of the AGB progenitor (spun
  up in a binary system or during a stellar merger).
In any event, a close binary evolutionary stage is indicated.
Unfortunately, ABL were unable to find further evidence that the
  central star is currently a close binary, as no
  variability was seen over their 7-day HST/WFPC2 observing campaign.

In principle the X-ray emission from K648 might arise from either diffuse
  thermal emission from a large cavity inside the nebula, or point-like
  emission from the PN nucleus (PNN; see Soker \& Kastner 2002 for a
  recent review).
However, given its short-term variability (within 19 days), emission
  from the compact PNN is much more likely.
Soker \& Kastner (2002) predict that 20--30\% of elliptical PNe
  probably have magnetically active late-type companions in binary
  systems with $a\hbox{${_<\atop{\sim}}$} 65$${\rm R}_{\odot}$\space and X-ray luminosities of
  $L\hbox{${_>\atop{\sim}}$} 10^{29}$~erg~s$^{-1}$.
Indeed, the most likely scenario, in view of K648's X-ray variability, is
  some sort of binary system, where accretion either directly or
  indirectly is reponsible (J. Kastner, priv. comm.).

\section{Conclusions}

We have identified four faint X-ray sources in the globular cluster
  M15 using {\it Chandra}.
Three of these are probable DNe (although the possibility
that source B is a qSXT cannot be ruled out) and the fourth is
  associated with the planetary nebula K648.
One of the DNe (source A) was initially discovered by applying image
  subtraction to WFPC2 images of the core of M15 (Charles et
  al. 2001).
In this study we reported on the detection of its X-ray emission.
The qSXT/DN (source B) and the other DN (source C) were first detected
  using {\sc wavdetect} in the {\it Chandra} images
  and then associated with optical counterparts
  in HST images, which allowed us to speculate on their nature.
We have also discovered that the PN K648 in M15 (source D) is a variable X-ray
  source, perhaps indicating a binary nature for the planetary nebula nucleus.
If K648 is indeed the source of the X-rays, it
  is both the first globular cluster and the most distant
  X-ray detected planetary nebula.

Sources A, B and C (both DNe and the qSXT/DN)
  had X-ray luminosities ranging from
  $2.34\times10^{31} - 3.66\times10^{32} \ {\rm erg} \ {\rm s}^{-1}$ in
  the 0.5--7~keV range during these {\it Chandra} observations.
Converting the luminosities to the 0.5--2.5~keV range, one gets a
  minimum luminosity of  $3.11\times10^{31} \ {\rm erg} \ {\rm
  s}^{-1}$ and a maximum of $2.27\times10^{32} \ {\rm erg} \ {\rm
  s}^{-1}$ -- these luminosities place these sources at the bright end
  of the galactic systems studied by Verbunt et al. (1997).
This implies that the majority of DNe in M15 remain to be
  discovered by more sensitive observations.
In order to identify optical counterparts of more {\it Chandra} sources,
  we need deeper imaging of M15 (to identify very faint sources like qSXTs or
  magnetic CVs), as well as observations at different epochs (to catch
  quiescent DNe and X-ray transients in outburst).

\section*{Acknowledgments}

DCH is grateful to the Academy of Finland and to PPARC for financial
support. MBD gratefully acknowledges the support of a Swedish Royal
Academy of Sciences (KVA) Research Fellowship.
The authors thank Craig Heinke, Bruce Balick and Joel
Kastner for valuable comments.
The authors also wish to thank Jonathan C. McDowell for useful
suggestions, Miriam Krauss at the {\it Chandra} HelpDesk,
and the anonymous referee for useful comments.
DCH is grateful to Panu Muhli for useful comments.
This research has made use of NASA's Astrophysics Data
System, SAOImage DS9, developed by Smithsonian Astrophysical
Observatory, and of the SIMBAD database operated at CDS, Strasbourg, France.
Based on observations made with the NASA/ESA Hubble Space Telescope,
obtained from the Data Archive at the Space Telescope Science
Institute, which is operated by the Association of Universities for
Research in Astronomy, Inc., under NASA contract NAS 5-26555.

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\end{document}

redpajama_set_name: RedPajamaArXiv


text:
Major Offshore Potential In This Tiny Nation
By Editorial Dept - May 22, 2015, 4:15 PM CDT
The North Sea has long been in decline. An era in which the British Islands fueled Europe's oil and gas needs, which has lasted for over a generation, is slowly coming to a close.
But while Scotland (and thus, the UK) has been the base for North Sea oil development, Ireland has largely been left out of the hydrocarbon bonanza. Having never developed its own oil and gas resources, Ireland has been a sort of forgotten step child to its larger neighbor just across the Irish Sea.
However, that could soon change. A recent announcement about the large potential for oil and gas off the coast of Ireland is raising hopes that Ireland's day may finally arrive. For now, low oil prices will keep rapid development at bay. But when oil prices rebound, with some luck, Ireland may no longer stand in a British shadow in terms of energy development.
Offshore Ireland
Ireland has never been a significant player in the energy world. It faces some challenging exploration conditions, including rough Atlantic waters and drilling depths often between 500 and 2,000 meters.
Offshore Ireland has been a tough nut to crack. There have been over 200 wells drilled around Ireland, but only two of them have yielded commercial discoveries. Royal Dutch Shell (NYSE: RDS.A), with its partners Statoil (NYSE: STO) and Vermilion Energy (NYSE: VET), developed the Corrib gas field, a natural gas project off the northwest coast of Ireland. Even that had an…
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