text:
<?php

namespace NetSuite\Classes;

class AccountingPeriod extends Record {
    public $periodName;
    public $parent;
    public $startDate;
    public $endDate;
    public $fiscalCalendar;
    public $closedOnDate;
    public $isAdjust;
    public $fiscalCalendarsList;
    public $isQuarter;
    public $isYear;
    public $closed;
    public $apLocked;
    public $arLocked;
    public $payrollLocked;
    public $allLocked;
    public $allowNonGLChanges;
    public $internalId;
    static $paramtypesmap = array(
        "periodName" => "string",
        "parent" => "RecordRef",
        "startDate" => "dateTime",
        "endDate" => "dateTime",
        "fiscalCalendar" => "RecordRef",
        "closedOnDate" => "dateTime",
        "isAdjust" => "boolean",
        "fiscalCalendarsList" => "AccountingPeriodFiscalCalendarsList",
        "isQuarter" => "boolean",
        "isYear" => "boolean",
        "closed" => "boolean",
        "apLocked" => "boolean",
        "arLocked" => "boolean",
        "payrollLocked" => "boolean",
        "allLocked" => "boolean",
        "allowNonGLChanges" => "boolean",
        "internalId" => "string",
    );
}


text:
'WCup was about tactical discipline'
Published:Wednesday | July 18, 2018 | 12:00 AMLivingston Scott/Gleaner Writer
France's teenage star Kylian Mbappe (10) scores against Argentina during their FIFA World Cup round of 16 match on June 30. France won 4-3 to eliminate Argentina.
Ricardo Makyn
Local coaches Shavar Thomas, Omar Edwards, Vassell Reynolds have described the 2018 World Cup as one which was a fantastic spectacle, full of suspense and unpredictability.
According to the coaches, the smaller nations came to the fore in a big way and they believed that was possible because of the tactic of playing behind or without the ball for the majority of their games. Local teams, they said, can learn a lot from this tactic.
Tivoli's coach, Edwards, said the smaller European teams were 'pragmatic' in their approach and local players and teams have to learn to be more disciplined if they want to compete at the highest level.
"The teams in the World Cup were compact and organised from the first whistle. Most played a low press game. They were very cagey, so most teams played on the counter-attack. It's not new, we have been doing a long time but the teams in the World Cup reinforced it," he said.
He added that team discipline cannot be achieved without individual discipline, which is not strong enough in domestic competitions.
"We have taken note of tactical discipline of the players to carry out coaches' instructions. They were very disciplined for the most part and organised, especially the European teams. So if our local players want to play at the highest level, if teams want to play at the highest level tactically, players have to learn the game more and be more disciplined," he said.
Thomas, the coach of Red Stripe Premier League (RSPL) champions, Portmore United, agreed the World Cup reinforced how effective playing behind the ball or without the ball is, while using the counter-attack to break open opposing defences.
"You take something from each team, especially, the way they played behind the ball and the patience they had. Small European teams - Iceland, Sweden and Denmark - were comfortable without the ball and were very happy and willing to defend.
"In the final Croatia had more possession but France were more effective in executing their plan. So you never know what can happen on the day, but this is football ...," he reasoned.
Vassell Reynolds, of Reno and daCosta Cup winners Rusea's High, said the World Cup taught him to be pragmatic and to adjust to situations.
"I didn't want to get caught up with supporting (Argentina) and get emotional. I really wanted to learn during this World Cup," he said.
"What I recognised this World Cup is that you can be pragmatic as a coach to counter what you think your opponents will be doing. I thought Belgium and England showed that in many instances. So you can be pragmatic during a tournament, during a game and not just go in there with one plan
"But this World Cup people (teams) were not just about or bent on defending ... they countered. So they were more adventurous," he stated.
«Sambo team flies out today for Pan Am Champs
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redpajama_set_name: RedPajamaCommonCrawl


The rubidium atomic clock requires an accurate time source to initially set the time. Originally I used a RS232 GPS puck but I then looked for something home grown. The answer was to use sime NTP Client to obtain the time from an internet time server and send the date and time as text to the atomic clock.
This simple NTP client uses a w5100 ethernet chip and a mega32 for its intelligence.
This site may be personal technical tutorial site about AVR tech.
in this site, there are 3 ethernet module for prototype.
2 are W5100 based modules and 1 is ENC28J60 module.
He also wrote useful example for network moudle like "NTP Client".
but we're afraid, there is no source code.
however he opened the hardware schematic.
The Eagle files can be downloaded here.


text:
Opens with a fresh fruit character on the nose and the sweetness is balanced with a citric zesty quality. The palate remains sweet and develops to a crisp Malty and gently spiced character. The finish is medium-long, still softly spiced with more of that fruity sweetness.
Established in 1947, Douglas McGibbon & Co is an independent, family owned company in our third generation who pride ourselves on taking a hands-on and artisan approach to our Single Grain Scotch Whiskies.
We believe Scotch Whiskies and people are similar in many ways. Both display complex characteristics which evolve and change over the years. From youth to maturity, impacted on by nurture and nature. Like people, no two Single Grain Scotch Whiskies, especially those from Single Casks, are identical.
The first sip of our Single Grain Scotch Whisky reveals a rich life-story. Unveiling moments from the past, and transporting us through the ages on our journey to the present. Today's rain drops will eventually flow into tomorrow's stills, then into casks that will sleep silently under untold moons before finally finding themselves in a treasured dram years later...
In our Clan Denny range, we hope you will find friends of many different characters and ages. Each has a slightly different story to tell, from still to cask, to dram, but with one thing in common; these Whiskies have all been hand selected from the Douglas McGibbon family stocks, and presented to you without colouring or chill-filtration...
Completely full of individuality!
Distilled: April 2007
Bottled: June 2017
Number produced: 450 bottles
Clan Denny Glengoyne 2007 10 year old


Yesterday afternoon the sun poked through the smoky ash and fog hanging over Carmel, to give an orange cast to objects below in our house.
The Soberanes Fire has consumed 23,000 acres and destroyed 20 homes. Yesterday, fire officials said the blaze is 10 percent contained and may not be put out until August 5th. I've posted many photos this year of the Soberanes area, including a canyon trail that leads to old growth redwoods, about six miles from our house. I assume these majestic trees are no more. More than 2,300 firefighters have been battling this fire. We thank them for their courage and pray they stay safe.
Carmel at noon yesterday was covered in smoky fog.


Agenesis of lateral maxillary incisors can be treated by two alternative options: Closure of the spaces followed by reshaping of the canines that will be functioning as laterals, or maintenance of the spaces with replacement of the lateral incisors with an implant after presumed cessation of the development of the alveolar process. The first treatment choice is preferable when the shape of the canines allows for an acceptable reshaping, the premolar root allows for a suitable crown torque and the space closure will not have a detrimental effect on the patient's profile. If any of these preconditions are not fulfilled a replacement is indicated. As a bridge requires an intervention on the adjacent teeth the implants seem to be preferred [1,2].
While waiting for growth to cease,temporary replacement of the missing tooth by a removable plate with a tooth or a bonded bridge with or without preparation of adjacent teeth have been suggested.The disadvantage of the removable plate is obviously the demanding compliance in addition to the continuously coverage of the palatal mucosa. The adhesive bridge will often have a limited retention or require invasive procedures in healthy teeth. In addition several papers have demonstrated a significant decrease in both width and height of the alveolar ridge in patients with congenitally missing a maxillary lateral incisor who received orthodontic treatment to create space for a dental implant [3,4].
To overcome these problems TADs were suggested as a basis for temporary replacement of lateral incisors.5-9 Vertical insertion of TADs on the top of the edentulous area did on the other hand not allow for the the vertical development of the alveolar process as they did not follow the eruption of the adjacent teeth. The present paper shows an alternative method which can be used as semi-permanent replacement of the missing incisors. The approach allows for the maintenance and development of the alveolar process until maturity has been reached in the patients where a missing tooth is meant to be replaced by an implant at adult age [10,11].
After a mild infiltration anesthesia, an Aarhus mini-implant®[i] with a bracket-like head and a high collar is inserted perpendicular to the alveolar process palatally in the edentulous area, approximately corresponding to the coronal third of the length of the roots of the adjacent teeth.
The construction of the pontic was performed chair side the day of the insertion of the mini-implant without no lab procedure ( Figure 1).
Figure 1A. Insertion of mini-implants.
Figure 1B. Configuration of the wire.
Figure 1C. Final insertion of the pontic.
Figure 1D. Initial frontal introral view.
A 0.021x0.025 SS sectional wire is inserted into the slot of the mini-implant and ligated tightly by a metal ligature. The wire is extending from the miniscrew to the top of the edentoulus alveolar process where it is configurated so that it can generate retention for the composite shaped as a crown. A metal primer[ii] is applicated to the wire and dried for 2-3 seconds followed by application of a bonding agent[iii] which is light-cured for 40 seconds.The crown replacing the missing tooth is formed coarsely by adding layer after layer of composite[iv] around the extension of the wire, polymerized for 20 seconds each time,starting from the gingival side, working labially and occlusally until the build up of the lateral incisor is accomplished.
In order to complete the gingival and lateral surfaces of the pontic, the wire with the pontic is loosened from the miniscrew , finishing is done extraorally and checked in the mouth until both form and function are acceptable.Then the pontic is refined with fine diamond burs and silicon points and finally ligated tightly to the bracket-like head of the mini- implant. At the end a fluid composite[v] is applied over the head of the screw for comfort of the patient.
Following insertion it is crucial that the patients are instructed in flossing daily between the pontic and the mucosa. The passage of the floss under the pontic also ensures that no pressure is added to the edentulous alveolar process.
As retention for the orthodontic tooth movement, performed for the opening of the space for the missing upper lateral incisor, the canine and the central incisor are splinted with the adjacent teeth and not with the pontic that remains separated.
The temporary replacement of missing maxillary lateral incisors have been followed up to 5 years from the insertion. The patients were seen every 6 month and the wire adapted so that the heigth of the pontic followed the eruption of the adjacent teeth and did not exert continuous pressure on the top of the aveolar process .The soft tissues adapted well to the pontic over the years. No inflammation of the soft tissues around the pontic was detected, most likely due the facility of dental flossing in this area. The intermittent pressure exerted to the central part of the mucosa during function might have contributed to the generation of papillae between the pontic and the adjacent teeth.
Inflammation of soft tissues around mini-implants did sometimes occur but it disappeared increasing oral hygiene and daily chlorhexidine mouth rinses.
No bone resorption around mini-implants was noticed and the vertical development of the alveolar process followed the eruption of the adjacent teeth. The intermittent tipping moment generated with respect to the screw when the pontic was loaded during biting was well accepted and may have contributed to the maintenance of the density of the alveolar bone.12None of the mini-implants were lost.
A possible rare complication was breakage of the ligature wire which was then substituted by a wire of a larger dimension.
Gingival impingement will occur when the adjacent teeth erupt more than the distance between the pontic and the mucosa . The maintenance of a distance between pontic and alveolar mucosa is however extremely important in order to allow for a continuous vertical development of the alveolar process . Moving the pontic more occlusal can easily be done by straightening the wire connecting the pontic with the mini-implant. A small V bend on the wire when constructing the pontic allows for the adjustment without removal of the wire from the bracket head of the mini-implant.
In our sample some mini-implants were inserted bicortically. In CBCT images at 5 year follow-up control it was noticed that the buccolingual width of the alveolar process had been totally preserved during growth (Figure 2). In addition,the described technique to replace the missing teeth also facilitates the later insertion of a dental implant as it maintains both morphology and density of the alveolar bone in that region .
Figure 2A. Initial sagittal cone-beam section of the alveolar process.
Figure 2B. Sagittal cone-beam section at 5 year follow-up.
Based on these observation it can be recommended to assess the thickness of the alveolar process on a CBCT of the patient or by measuring the thickness of the alveolar process and mucosa directly in the mouth so that the length of the threaded part of the mini-implant corresponds to the horizontal dimension of the alveolus. Based on these measurements a surgical guide will ensure the correct insertion of the mini-implant.
The present report describes a solution to the replacement of missing maxillary lateral incisors. The method is compliance free, requires no invasive intervention on the adjacent teeth and allows for the normal development of the alveolar process both in height and width. It is not limited to a specific age and can possibly also be used as a temporary solution during a prosthetic reconstruction phase .
Zachrisson BU, Rosa M, Toreskog S (2011) Congenitally missing maxillary lateral incisors: canine substitution. Point. Am J Orthod Dentofacial Orthop. 139: 434, 436, 438.
R.Ciarlantini,B (2017) Melsen Semi-permanent replacement of missing lateral maxillary incisors by mini- implant retained pontic: A follow-up study. Am J Orthod Dentofacial Orthop 151: 989-94.
©2018 Ciarlantinia R. This is an open-access article distributed under the terms of the Creative Commons Attribution License, which permits unrestricted use, distribution, and reproduction in any medium, provided the original author and source are credited.


text:
class CommandSendBlocking : public ICommandHandler
{
	thread::Mutex count_mutex;
	thread::Condition count_threshold_cv;
	volatile bool received;
	eCommand command;

	static const long timeOut = 10; // Timeout in seconds

	virtual bool Handle(Command& cmd, ICommandHandler* source);

public:

	Command*  m_Response;

	CommandSendBlocking();
	virtual ~CommandSendBlocking() {}

	bool SendBlocking(const Command& cmd, ICommandHandler& dest, CommandDispatcher& disp);
};

#endif // COMMANDSENDBLOCKING_H_

redpajama_set_name: RedPajamaGithub


Maybe you have been feeling overwhelmed by all the things on your to-do list. You might even find yourself holding your breath and rushing off from one thing to the next without even noticing. This time of year, in particular, you might feel like you are being swept up by all that you have to get done.
I recently shared some information on how we have become wedded to our busy lifestyles and never-ending to-do lists. For many of us, success and status are measured by how busy we have gotten and yet, we often wish we could slow down.
One of the challenges has become wanting to accomplish it all and yet slowing down the pace. While this might seem like an impossible feat, there are ways of slowing down while enhancing our productivity and performance. This way, we are not bombarded by feelings of shame, guilt, fear, and overwhelm so that we can still accomplish what we value and spend time relishing components of our lives that allow us to recharge. We can find ways to be more present in our relationships and also nurture our own physical and emotional well being – and, in turn, the areas we invest our energy into become turbo charged as well.
Read on for some tips on helping yourself become more skilled at improving your productivity!
Please share your experience with me – leave a comment and let me know your thoughts on how you slowed down your go-go-go schedules while focusing on the life you want to celebrate!


Soft fine tynex nylon bristles.
Flexible rubber neck and wide oval head reduce the pressure of brushing.
Available in right or left hand orientation with a ergonomic non-slip grip for accurate and effective brushing.
6,000 premiun fine Tynex nylon bristles (over 3 times more than ordinary toothbrushes) efficiently massage the gums and effectively clean teeth at the same time while providing a softer brushing experience overall.
Reduce Waste - 60% of our users report it lasting three times longer than ordinary toothbrushes. Rinse with peroxide to clean after 3 months.


One of my favorite artists, and a familiar face here at Fresh Fruit, makes a grand return with his latest single Changes. This time around Atm absorbs bakkwoods relaxed and sampled production, speaking on his future plans and expectations softly for an entertaining two and a half minutes. If you have followed him up to this point you will definitely enjoy this track. Keep an eye out for his next release and check out the new single below.


· Belinda has been in the wine industry for over 20 years after discovering her life's passion in Bordeaux. She has worked across Europe and New Zealand in all aspects of the trade, including selling, buying, educating, marketing and making wine. As well as director of the Liquorland Top 100 International Wine Competition, Belinda is also a consultant to various wine producers.


text:
Now reading: Our Second Skin Studio & Lab is Opening Soon!
Our Second Skin Studio & Lab is Opening Soon!
We're family owned, grass roots, born and raised in Wisconsin, and we're growing.
Our first location in Cross Plains, Wisconsin is where it all started. Behind closed doors, tucked in the woods, it was two years of formulating, researching, developing, and starting over before we had our 40 products to share in 2013.
Two years later, almost to the day, we were thrilled to be opening our lab and Skin Studio in Cross Plains, Wisconsin. It's in the heart of the community where we were living, and it's all about being able to reach out and build relationships with our new friends, neighbors, and customers.
Now, it's 2017 and we're circling back to where our family first started, and the place where it has always felt like a second home… San Clemente, California.
We found a little fixer-upper boutique right in the shopping district of San Clemente on Avenida del Mar. We're happy to say that our plans have been approved, the permits have been given, and we're making progress in our space.
Electrical – done. Plumbing – done. Drywall – done. Paint… getting started. Next the floors, trim, ceiling, and lighting.
Then, the fun begins. We're bringing in all of the organic ingredients and botanicals that we need to make our fresh, proprietary treatments to share. Delight!
It's a lesson in patience and progress. Just like our hand-crafted and small batch treatments… good things take time. A home cooked meal, an exercise plan, and following a healthy self-care ritual. All of these things take time.
You put the time in, and you'll receive the rewards.
Modern Luxury Magazine Buzzing about our New CA Location
In Between Washes? No time? No problem.


text:
elodie-meheust » Funk » Brook Benton - Rainy Night In Georgia
Brook Benton - Rainy Night In Georgia album download
Brook Benton Soul Rhythm and Blues Vocal 1996 UK
Performer: Brook Benton
Title: Rainy Night In Georgia
Style: Soul, Rhythm & Blues, Vocal
Format: MP3 FLAC MPC VOC MP1 VOX RA MP4 WAV
Genre: Funk / Blues / Pop
Rainy Night In Georgia.
Rainy Night in Georgia" is a song written by Tony Joe White in 1967 and popularized by R&B vocalist Brook Benton in 1970. It was originally released by White on his 1969 album, Continued, on Monument Records, shortly before Benton's hit single was issued. In a January 17, 2014 interview with music journalist Ray Shasho, Tony Joe White explained the thought process behind the making of "Rainy Night in Georgia" and "Polk Salad Annie".
Album Brook Benton Today. Rainy Night In Georgia Lyrics. Hoverin' by my suitcase Tryin' to find a warm place To spend the night Heavy rain fallin' Seems I hear your voice callin' It's all right. A rainy night in Georgia A rainy night in Georgia It seems like it's rainin' all over the world I feel like it's rainin' all over the world. Neon signs a-flashin' Taxicabs and buses Passin' through the night A distant moanin' of a train Seems to play a sad refrain To the night. I find me a place in a boxcar So I take my guitar To pass some time Late at night when it's hard to rest I hold your picture to my chest And I feel fine, I. But it's a rainy night in Georgia Baby, it's a rainy night in Georgia I feel it's rainin' all over the world Kind of lonely now And it's rainin' all over the world Oh, have you ever been lonely, people?
Christmas With Brook Benton. Brook Benton Selected Hits (Vol. 3). 2006. 2). 1999. 1). Hi-Five: Brook Benton - EP. 2007.
Album: Brook Benton Today (1969). Charted: 4. Get the Sheet Music License This Song. Hoverin' by my suitcase Tryin' to find a warm place to spend the night A heavy rain a fallin' Seems I hear your voice callin' "It's all right". A rainy night in Georgia A rainy night in Georgia I believe it's rainin' all over the world. Neon signs a flashin' Taxi cabs and busses passin' through the night The distant moanin' of a train Seems to play a sad refrain to the night . And on March 8th, 1970 it reached (for 1 week) on Billboard's R&B Singles chart.
Features Song Lyrics for Brook Benton's Rainy Night In Georgia - Greatest Hits album. Brook Benton - Rainy Night In Georgia - Greatest Hits Album. Artist: Brook Benton. Send "Brook Benton" Ringtones to your Cell. Album: Rainy Night In Georgia - Greatest Hits.
Download MP3. Brook Benton. Dinah Washington, Brook Benton. It's Just A Matter Of Time.
Rainy Night In Georgia 4:06
Think Twice 2:52
The Same One 2:20
Hotel Happiness 2:37
So Many Ways 2:31
Endlessly 2:29
Revenge 2:28
Thank You Pretty Baby 2:26
Lie To Me 2:12
Kiddio 2:37
The Boll Weevil Song 2:50
Baby (You've Got What It Takes) 2:57
My True Confession 2:36
It's Just A Matter Of Time 2:30
A Rocking Good Way (To Mess Around And Fall In Love) 2:29
Frankie And Johnny 2:27
It's Just A House Without You 2:31
I Got What I Wanted 3:01
For My Baby 3:10
So Close 2:04
303162 Brook Benton Rainy Night In Georgia (CD, Album) Hallmark Records 303162 UK 1996
CD6103 Brook Benton Rainy Night In Georgia (CD, Album) Music Digital CD6103 UK 1997
Related to Brook Benton - Rainy Night In Georgia
Brook Benton With The Merry Melody Singers - Hotel Happiness album mp3
Brook Benton - Hotel Happiness album mp3
Brook Benton - Fools Rush In / The Boll Weevil Song album mp3
Brook Benton - Something For Everyone album mp3
Randy Crawford - Rainy Night In Georgia album mp3
Brook Benton - Kiddio album mp3
Tony Joe White - Rainy Night In Georgia / Willie And Laura Mae Jones album mp3
Brook Benton - I Wanna Be With You album mp3
Twa Toots - Please Don't Play 'A Rainy Night In Georgia' album mp3
Brook Benton, Charlie Francis - Brook Benton Sings (with Charlie Francis) album mp3


text:
UK political chaos over Brexit leaves Europeans bemused
by Adam Becket
'No one is happy' — bishops react to Brexit manoeuvres
The Prime Minister in the House of Commons on Monday, backed by members of her party, outlining the reasons for deferring a vote on the EU Withdrawal Agreement
The Prime Minister in the House of Commons on Monday, backed by members of her party, outlining the reasons for deferring a vote on the EU Withdrawal ...
EUROPEAN leaders are bewildered by the antics of the UK Government, the Bishop in Europe, Dr Robert Innes, said this week.
Speaking on Tuesday, after the postponement of a Parliamentary vote on the EU Withdrawal Agreement, Dr Innes, said: "It is very bewildering for Europe. My European friends cannot understand what is going on in the UK. I find it very sad to see my country in this state of confusion."
On Wednesday, the uncertainty deepened, despite the victory of Theresa May in a vote of no confidence in her leadership, triggered by the filing of 48 letters critical of her to the 1922 Committee.
In the result, 200 Conservative MPs backed the Prime Minister; 117 voted against. After the vote, Mrs May spoke outside No. 10, saying that it was time for her party to "come together in the national interest". But the size of the opposition to her Brexit strategy within her own party remains a stumbling block for the deal that she has been promoting.
The trigger for the no-confidence motion was the cancelling of the Parliamentary vote on the Brexit deal. She announced on Monday afternoon that, since it was clearly heading for defeat "by a significant margin", she was deferring the vote.
Her intention, she said, was to seek clarification from her European counterparts in an attempt to salvage the deal. When challenged in the Commons about whether anything in the deal would be changed, Mrs May only repeated that she was looking for clarifications and assurances. The European Commission President, Jean-Claude Juncker, said later that there was "no room" for renegotiation.
The Brexit vote could now be delayed until 21 January, it has been suggested.
Dr Innes said that a no-deal scenario would be "disastrous. . . We are in uncharted territory, it is hard to see where we will go now. I don't think the EU27 will renegotiate the withdrawal agreement, although the Prime Minister could get some clarifications. . . It would be irresponsible for the Government to drift towards a no deal."
The Bishop of Leeds, the Rt Revd Nick Baines, also expressed his despair at the week's proceedings. Speaking on Wednesday, he said: "The infighting within the parties in Westminster seems to relegate the national interest to a secondary matter. Surely it's time to identify a different narrative that holds the country together."
As for the future of Brexit, Bishop Baines said that it was "impossible to see what will happen next". Anyone who purported to know what would happen next was a "fantasist or a liar".
Like other bishops we spoke to, he was adamant that no deal was not an option. "The one thing that is pretty strong across the Commons and the Lords is that there can't be 'No deal'."
The Bishop of London, the Rt Revd Sarah Mullally, also spoke about the need for co-operation. She said on Tuesday: "The discussions around Brexit are not simply about legislation — they are about identity and the type of society we want to be. The EU referendum exposed divisions in our society, and the present political process risks deepening them.
"These divisions cannot be resolved by legislation — strengthening relationships amongst our communities is the key. Whilst I hope that politicians co-operate across party boundaries to find a way forward in the common good, I also hope that churches lead the way to build communities which are integrated and strong."
Bishop Baines has spoken favourably about a second referendum in the face of a parliamentary impasse (News, 23 November). The Bishop of St Albans, Dr Alan Smith, disagrees. He said on Tuesday that he did not think that a second referendum would solve anything. "Part of the difficulty is, following the [2016] referendum it is becoming clearer and clearer that what looked like a simple choice has been interpreted in many different ways.
"Nobody is happy now, and there is no consensus as to the way forward." Mrs May was in "a very difficult position".
Dr Smith said that he had been planning to support the Prime Minister's deal "in broad terms — because it is bound to involve some sort of compromise: as with all divorces, the problem is that neither side walks away happy".
He went on: "We need to have a realistic view that there will be other people wanting to get things out of this, and it will mean compromise."
His words were echoed by the Bishop of Lincoln, the Rt Revd Christopher Lowson. Although he voted Remain, his diocese voted Leave. He said on Wednesday: "It would seem that, as a nation, we have forgotten what compromise means." It was essential to find a new way to work together, "wha—tever one's personal opinions".
'No one is happy' — Bishops react to Brexit non-vote
ANYONE who purports to know what will happen next with Brexit is a "fantasist or a liar", the Bishop of Leeds, the Rt Revd Nick Baines, has said
The Bishop of Chester, Dr Peter Forster, said on Tuesday: "I hope that modifications, in some form, can be achieved, which will enable the proposed deal to go forward. Given the 52-48 split in the Referendum, a fairly soft Brexit seems to me to be the right way forward, if it can be enacted in a principled way."
The Bishop of Oxford, Dr Steven Croft, urged politicians "to look to the national interest, and not have belief in turning the clock back.
"As the Church, we need to be praying for the nation and for our politicians. We need to be saying to them 'please act in the national interest', because there are other more important issues that are being ignored."
Arguments continue to focus on the Irish border. In a letter to the Church Times this week, the Archbishop of Dublin, Dr Michael Jackson, pledges that the Church of Ireland would continue to function as a cross-border organisation.
"It is the duty and the opportunity for members of the Church of Ireland . . . to continue to contribute, not least in Brussels and elsewhere, to the sorts of encounters around civic and cultural issues proffered in the EU treaties and through the European institutions."
The Roman Catholic Bishops' Conference in England and Wales has criticised the proposed government settlement scheme to allow EU citizens to remain in the UK. A statement said on Wednesday: "We strongly oppose the decision to charge people for securing the rights they already have. This is not only unprincipled but will also create a barrier for larger families or people facing financial difficulties."
Bishop of Leeds defends amendments to the Government Brexit Bill
Lords force another Brexit defeat on the Government, after Northern Ireland fears
Gibraltar Brexit wrangle opens old wounds
Bishop of Leeds joins Lords defeat of latest Government Brexit Bill
Brexit Bill passes after Lords' amendments fail
Survivor on national safeguarding panel slams Birmingham diocese over redacted report
Survey on conversion therapy opens
Baptismal ritual may mark gender-change
Anti-Semitism on rise in Europe, says study
Ringer, 100, leads his birthday quarter-peal
WorldCommentFaith
Yorkshire and Lincs
Do you have a strong vocation to lead and manage a committed team of staff and volunteers, live as part of a healing, ecumenical community and be alongside our guests as they respond to loss, sorrow, and pain by finding new hope? People turn to us at times of trauma and transition to find their own strength, and we offer a holistic and sacramental approach based on justice, peace and ecology.


After its successful debut in 2018, the Techstars Dubai Accelerator in partnership with GINCO will host its second class in 2019 starting on 20th of January and Demo Day held on the 18th of April. Our second year of operation will continue the world class mentorship-driven programming in partnership with GINCO Investments and will be located at the brand new facilities of the Dubai Future Foundation's Area 2071, a visionary government initiative, at the iconic Emirates Towers.
Our program is agnostic to any industry sectors and has a special theme around 'Smart Cities'. Our definition of 'Smart Cities' is broad: covering enterprise software, logistics, mobility, industrial, e-commerce, smart energy and environment that are scalable anywhere in the world.
We are looking for exceptional founders, from all corners of the globe, who may be enterprise-ready or not, but are nevertheless tackling the mundane to the big, important problems with the use of disruptive solutions.
Founders that are developing leading edge technology for future smart cities, and the use of applications such as IOT, artificial intelligence, virtual or augmented reality, big data, machine vision, blockchain, or even quantum physics are encouraged to apply.
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text:
\section{Introduction}

The {\it EGRET}\  telescope on the Compton Gamma Ray Observatory
({\it CGRO}) satellite detected 271 sources in a survey of
the $\gamma$-ray ($\sim$100 MeV to 10 GeV) sky.  Counterparts for
the majority of these sources have remained elusive, and until
recently, roughly one quarter of these had been identified as
blazars \citep{har99,mat01}.  By adopting a new
technique, we have now pushed the identified fraction to
$\sim$70\% above decl. $> -40^\circ, \vert b \vert > 10^\circ$,
excluding the Galactic bulge (Sowards-Emmerd et al. 2003,
hereafter SRM03; Sowards-Emmerd et al. 2004).
The Large Area Telescope (LAT) on the Gamma-ray Large Area
Space Telescope ({\it GLAST}) satellite, scheduled for launch in
early 2007, is predicted to detect over an order of magnitude
more blazars than its predecessor.  The improved
sensitivity and resolving power of the LAT will provide
more accurate source positions; however, the fainter sources will
still only be localized to 5-10 arcminutes.  {\it GLAST}\  will be
instrumental in verifying the questionable {\it EGRET}\  detections but will
present an even larger set of its own marginal
or unidentified $\gamma$-ray detections.  The current
literature is lacking in well studied sources that would be
realistic counterparts for the thousands of new {\it GLAST}\  detections.

Blazars are jet-dominated active galaxies viewed
close to the axis of a relativistic jet.  Blazar
emission spans the entire range from radio to
$\gamma$-rays and is often observed to be highly
variable.  High-energy emission is thought to be the
result of synchrotron self-Compton (SSC) upscattering \citep{up95};
additionally, Compton upscattering of seed photons originating
outside the jet is often invoked \citep{bot02}.

Under the current classification scheme,
blazars are divided into two classes: flat spectrum
radio quasars (FSRQs) and BL Lacartae objects (BL Lacs) \citep{up95}.
According to the current zoology, BL Lacs are a
less luminous, more local population, drawn from a
parent distribution of elliptical galaxies.  FSRQs,
drawn from a quasar parent distribution, are generally
higher power sources and are visible to much
higher redshift.  Both classes typically exhibit compact
radio cores with flat radio spectra ($\alpha < -0.5$, where
$S_\nu\propto\nu^{-\alpha}$).

To aid in the counterpart identification of {\it GLAST}\  detections, we
have created a blazar survey that seeks to identify a number
of flat spectrum radio sources comparable to those expected from
extrapolation of the 3EG \citep{har99} detections.  We select targets
by applying our Figure of Merit (FoM) analysis, described
in detail in SRM03, to objects in the Cosmic Lens All-Sky Survey
(CLASS).  Excluding known 3EG counterparts, we have
compiled a source list of 710 $\gamma$-ray blazar
candidates.  The radio and X-ray properties of these
sources are very similar to those of the 3EG blazars, and
many are as bright or brighter in the radio.  As blazars
are highly variable in $\gamma$-rays, we expect that many of
these were simply inactive (in a `low state') when observed by
{\it EGRET}.  We have found archival identifications and
redshifts for nearly half of these sources in the current
literature, and the remainder are being observed at
McDonald Observatory.  We have contributed 241 new
spectroscopic identifications in this paper.  This means
that this northern sample is currently 74\% identified.

To further motivate the blazar nature of the survey
sources, we have searched the current release of the {\it EGRET}\  data
for excess flux at the radio source positions.  To this end,
we have developed two
methods to rank $\gamma$-ray detections statistically
in the {\it EGRET}\  data.  As a reality check on our technique,
we calculate the equivalent significance of a subset of the 3EG
sources.

The selection criteria of the blazar candidate survey are outlined
in Section 2.  The methods used to convert the {\it EGRET}\  Test
Statistic (TS) into a probability for an individual observation
and to combine these observations into an overall significance of
a $\gamma$-ray detection are described in Section 3.  In Section
4, these two methods are applied to 3EG sources, survey sources,
and the background sky.  A discussion of the merits of the
two methods also appears there.  Section 5 details the
spectroscopic observations of survey blazars.  Finally, Section 6
presents a rudimentary comparison between the 3EG blazars and the
blazar candidates presented in this survey.

\section{Survey Selection}

\subsection{Figure of Merit Selection}

By comparing the properties of radio sources located within 3EG error
ellipses (95\% confidence contours) to the background distribution, we
have developed a new method of ranking counterparts of {\it EGRET}\  $\gamma$-ray
sources.  We believe that previous analyses relied too heavily
on single dish 6 cm radio fluxes.  The recent release of the 8.4 GHz Cosmic
Lens All-Sky Survey (CLASS) \citep{mye03} in the north provided uniform
coverage over much of the northern sky.  In
addition to more accurate core fluxes, non-simultaneous one-to-one
spectral indices can also be extracted from the CLASS by pairing it with the
1.4 GHz NRAO VLA Sky Survey (NVSS) \citep{con98}.  This
mitigates the confusion in matching between the older single dish radio
surveys and improves the spectral index determination.  Fluxes for CLASS
sources were assigned by selecting the brightest source in each pointing
and combining all the flux within a 1'' radius to include any compact jet
features.  These CLASS sources
were matched to the NVSS positions with a 4'' match radius.  Based on the
number of sources in our survey, we expect on the order of one spurious
match.  Finally, the
{\it ROSAT}\  All-Sky Survey (RASS) catalogs were also integrated into this data set
to provide additional leverage in finding blazars.

Examining these surveys in the context of 3EG, we quantified the
correlation between flat spectrum radio sources and 3EG contours
(SRM03), which took the form of a fractional excess, $n$, of
sources (in a given flux or spectral index bin) found within the
3EG positional 95\% confidence contours relative to the random
background sources:
\begin{equation}
n = \frac{N_{\rm 3EG} - N_{\rm Random}}{N_{\rm 3EG}}
\end{equation}
\begin{equation}
{\rm FoM} = n_{\rm 8.4 \, GHz} \times n_{\alpha} \times n_{\rm X-ray} \times {\rm Positional \,\, Dependence}
\end{equation}
where these functions are defined as:
\begin{equation}
n_{\rm 8.4 \, GHz} = -3.47+2.45 {\rm Log}_{10}(s_{8.4})-0.34 [{\rm Log}_{10}(s_{8.4})]^2
\end{equation}
\begin{equation}
n_\alpha = {\rm Median}[0, 0.19-0.35\alpha_{8.4/1.4}, 0.4]
\end{equation}
\begin{equation}
n_{\rm X-ray} = 0.5+ {\rm Median}[0, 0.49+0.41{\rm Log}_{10}(cps), 0.5]
\end{equation}
The full analysis is described in detail in SRM03, including the positional
dependence.

Using the FoM method of selecting blazar candidates, we have created
a survey tailored to find objects similar to the 3EG blazars.
Radio candidates were selected from the 3.5 cm CLASS.  In this work, we
exclude the positional dependence of the FoM and select objects based only
on their intrinsic properties: radio flux, spectral index, and X-ray flux.
We have selected sources such that their FoM would meet our original
`plausible' ($<$18\% false positives) 3EG
FoM limits if the source were located on a 3EG 95\% contour.  This leaves
us with 710 sources selected from the CLASS survey that meet our criteria
and were not previously associated with 3EG sources.  Properties of these
sources are detailed in Table 1, the full version of which is available
in the electronic version. The FoM
selection effectively imposes a hard minumum on the CLASS radio flux
of $\sim$140 mJy.

\subsection{X-ray Selected Sources}

Before the CLASS data were available, we selected target sources as
an extension of the Deep X-ray Blazar Survey (DXRBS) \citep{per98} pushing
fainter in radio flux.  Sources were selected from NVSS/GB6/RASS matches
by the DXRBS criteria (keeping $\alpha<$0.7 and relaxing the flux cut).
This means that a RASS X-ray detection
was required for inclusion in the survey.  Application of the FoM
technique shows that these sources are not strongly
correlated with the 3EG positions.  Nevertheless, these sources are
generally legitimate blazars, and so we include their spectroscopic
properties for comparison.
We note here that several of the 3EG blazars
previously identified were not detected in the RASS,
which in part led us to drop the X-ray detection requirement.
Also, for high-power, low-peak blazars (FSRQs), the synchrotron peak
is generally in the optical/IR so that the X-ray band, lying between
the synchrotron and Compton components, can be quite faint.  In contrast,
the higher peak BL Lacs often show bright synchrotron X-rays, but are less
luminous in the GeV range.
Most of the X-ray selected sample does not make the
FoM cut since the radio fluxes are typically much fainter ($\sim$50 mJy)
than the FoM-selected sources.
For completeness, we tabulate redshifts and identifications in Table 2
for the X-ray selected sources that did not meet the FoM criterion.
Comparisons between properties of sources selected by this method
and by the FoM method are presented in Section 6.

\section{Analysis of the $\gamma$-ray Data}

To further motivate the $\gamma$-ray nature of our blazar candidates,
we investigate the possibility that
these blazars produce flux detected by {\it EGRET}\  but below the 3EG catalog
threshold.  This is done through a reanalysis of the
{\it EGRET}\  data products, cleaned of the 3EG sources.
We begin with the counts maps (photons), exposure maps, and maps
modeling Galactic foreground emissions from the current release
of the {\it EGRET}\  data products.  These maps exist with a wide range of photon
energy cuts. For this analysis we follow the standard procedure and
only employ the {\it E} $>$ 100 MeV data.
These data files are divided in time into individual `Viewing Periods'
(VPs), which are pointings typically spanning a few days to a few
weeks, and into `Cycles,' which comprise roughly
a year's worth of observations.  Maps were also
produced for all possible sequential combinations of these Cycles.

LIKE (v5.61 at the time of analysis) is the standard source
detection routine and was developed specifically for {\it EGRET}\
data \citep{mat96}.  LIKE computes a `Test Statistic' (TS) value
through a maximum likelihood technique that compares the likelihood
of detecting a source to the null likelihood (no source) for a
given position through fits to the aforementioned data files.  Source
positions, detection significances and fluxes can be extracted from
the likelihood maps created by LIKE by searching for peaks in the maps.
Once sources are detected, they can be modeled in the background or
`cleaned,' and these `cleaned' maps can be searched again for the peaks in
likelihood.  This procedure can be iterated down to a fixed TS threshold.

At present, the 3EG catalog represents the most thorough
analysis of the {\it EGRET}\  data collected during survey mode
(Cycles P1-P4).
Sources compiled in the 3EG catalog were selected by searching
combinations of the {\it EGRET}\  data for
any $\sqrt{\rm TS}\geq 4$ detections ($\sqrt{\rm TS}\geq 5$ required
for $\vert b\vert
<10^\circ$).  The blocks of data searched for excess $\gamma$-rays using LIKE
included VPs, a handful of combinations of sequential VPs, Cycles P1-P4,
and the combinations of Cycles P12, P34 and P1234.  For a detailed
description of the specifics of the 3EG catalog,
we refer the reader to Hartman et al. (1999).  However, this 3EG detection
threshold, required for inclusion
in the catalog, does not account for the number of trials examined
-- generally on the order of 15-35 -- nor does it account for the
increase in significance
associated with choosing the source position at the local TS
maximum instead of using the more accurate radio counterpart position.
Additionally, only sequential VPs
were coadded and analyzed, although a randomly flaring source might be expected to appear in disjoint VPs.

\subsection{Searching the {\it EGRET}\  Data}

From the previous analyses of the {\it EGRET}\  data, we believe the $\gamma$-ray
behavior of these blazars is often highly variable on timescales
down to at least the length of {\it EGRET}\  VPs.  Therefore, we select
the individual VPs as the building blocks for our
analysis.  However, we wish to avoid making
any unnecessary assumptions about the $\gamma$-ray properties of these
sources; that is, we do not want to be limited  to searching
for sources that exhibit a single flare or, conversely, are steady
in the $\gamma$-rays.

In our search for correlation between this survey and $\gamma$-rays
detected by {\it EGRET}, we chose to examine the significance of
$\gamma$-ray detections at the precise radio positions of sources.
Using radio positions avoids `peaking up' the source positions on
background fluctuations.  Obviously, this method generally returns a lower
significance detection compared to using the position where the
TS is a maximum ($\gamma$-ray position).  Therefore,
our detection significance represents a conservative lower limit
when compared with the 3EG rankings.  We believe this is the
proper method for computing the flux or significance of a detection for
{\it EGRET}\  data when a precise position is known for a candidate counterpart.

\subsection{Method}

We begin by analyzing the individual blocks of data: VPs ($\sim$few days),
Cycles ($\sim$year), and combinations of Cycles.  Details of the beginning
and ending dates and field centers of the VPs are summarized in Hartman
et al. (1999).
For each VP overlapping our region of interest,
we create likelihood maps from the {\it E} $>$ 100 MeV maps using
LIKE.  All 3EG sources in the field of view of a
given viewing period are modeled (fluxes fit, not fixed).  Only
data within $30^\circ$ ($19^\circ$ for the four `narrow-mode'
pointings) of the field center are included in the
analysis.  TS values representing the likelihood
of source detection at a given point can be read directly off
these $0.5^\circ \times 0.5^\circ$ gridded maps.

We analyze only the region covered by CLASS
($0^\circ <$ decl. $< 75^\circ$ and
$\vert b \vert > 10^\circ$).  Additionally, we remove the
Galactic bulge to a radius of $30^\circ$ from the Galactic center
due to the high density of 3EG
detections in the bulge.  Finally, regions of $2^\circ$ radius around
3EG sources were excluded from the analysis.  LIKE tends to oversubtract
sources when they are modeled, leading to an excess of low TS
values relative to a random background;  that is, when a point source
is modeled by LIKE, the resulting likelihood distribution in that
region is
not consistent with random background and is instead almost entirely
filled with
TS $<$ 1 values.   If sources were properly cleaned, one would expect
to find a random distribution (e.g., approximately one TS $\geq$ 4
($2\sigma$) point for every $\sim$40
points) where a source was modeled.  This oversubtraction problem
becomes insignificant at approximately 2$^\circ$ from {\it EGRET}\  sources.
A precise treatment of this issue would involve making cuts
around each 3EG source based on its flux in each individual
viewing period; however, we believe that a simple 2$^\circ$ cut is
satisfactory for the purpose of this work.  The subset remaining
after applying these cuts contains 578 of the original 710 objects.

\subsection{Converting TS into a Probability}

With TS values in hand, we require a means to transform a set of
TS into a meaningful probability of a $\gamma$-ray excess at a given
position.  We consider three approaches to
converting TS to a properly normalized
probability.  The trivial method employed in Mattox et al. (1996) is
simply to assume that TS is distributed like $\chi^2_1/2$.  From this,
one can simply convert via $\sqrt(\rm TS) \rightarrow \sigma$.
This predicts that
exactly 50\% of the data points in a blank field should have TS = 0.
However, in the
northern sky data cleaned of the 3EG sources, even excluding
2$^\circ$ around the positions of the 3EG sources,
we find $\sim$59\% of the points have TS = 0.  We believe that this
is largely due to overfitting of {\it EGRET}\  point sources and the free
normalization of the diffuse background flux.  This therefore
produces a large discrepancy in any analysis that includes
low TS values.  This method may be reasonable when applied
to large TS values; however, in searching for faint detections
it is clearly inadequate.

The following two methods treat the cleaned {\it EGRET}\  data as the starting
point and use the observed distribution of TS values to determine the
corresponding probability.  This is done by summing up the number of
positions in a given VP with TS greater than a given value and
normalizing this to the total number of points in the viewing period:
Prob($>$TS) = \#($>$TS)/\#(Total).
This probability function is only applicable to points in a single VP,
so this procedure is repeated for each VP and Cycle.
The overall number of positions in a VP is the
limiting factor here, and due to the spatial cuts listed above, this
number can be as small as a few hundred.
For small TS values, this method, while heuristic, is the most robust.

To extend the analysis to lower probabilities (larger TS), we can
concatenate the VP TS distributions and compute the probability
distribution for all VPs at once.  In doing this, we are able to increase the
number of points considered by two orders of magnitude, and
hence the resulting range of probabilities can be extended by a
comparable amount.  This approach averages out the VP-to-VP
variations in the low-TS end of the distributions.
This is checked by comparing with the results of the individual VP
method; little
difference is observed between the resulting final probabilities
for low-significance sources.  Thus, as one would expect, the background
fluctuations average out in the sets of overlapping VPs.
Since these differences do average out,
we chose to adopt this method because it allows the larger TS values to
be treated uniformly and it extends the probability range by two orders of
magnitude.  By selecting this
occurrence-based method over $\chi^2$, we are treating
the data as though we are starting from scratch with the
3EG-cleaned maps.  Examples of these distributions are shown
in Figure 1.

\clearpage
\begin{inlinefigure}
\figurenum{1}
\scalebox{1.0}{\rotatebox{0}{\plotone{f1.eps}}}
\figcaption{The distribution of TS for
seven individual VPs (gray) and the concatenation of
all 169 VPs (solid black).  This may be compared with the
$\chi^2/2$ distribution (dashed black).  Note the large discrepancy
between these distributions as TS approaches zero.  This effect
is averaged out in the concatenated distribution.  Additionally,
note the large variation in the maximum TS values found in
individual VPs.}
\label{Fig1}
\end{inlinefigure}
\clearpage

\subsection{Combining the Information}

For each test position, we now have a set of probabilities
corresponding to the individual VP observations.  Our task now is
to integrate these probability estimates into a single detection significance.
We investigate two methods.  The first method takes an agnostic
stance on the temporal behavior of a source and
combines all the information available on the VP timescale.
We believe that it should be possible to extract almost
all of the information available in the Cycle and combination maps by
combining information from the individual VPs.
We create the `combined' probability at a given position by multiplying the
individual VP probabilities in which that position was observed.  Clearly,
the resulting probability is strongly dependent on the number of VPs,
so we must renormalize.  We do so by integrating over the
volume of {\it N}-dimensional combined probability space where the combined
probability is less than or equal to that of the source.  That is, we
determine how likely it is to build up the combined probability in question
from {\it N} observations of random TS values.
This problem can be solved analytically, and the final,
normalized probability can be written as:
\begin{equation}
P_{\rm norm} = p \sum_{i=0}^{N-1} (-1)^i \frac{\ln^i p}{i!}
\end{equation}
where {\it p} is the product of VP probabilities at a given position.
Using this procedure, we can compare positions observed in different
numbers of viewing periods.  We designate this probability as the `Product'
probability.

In the second method, for each position, we create a set of TS
values extracted from the likelihood maps from VPs, Cycles,
and combinations of Cycles (P12, P34, P1234).  We include combinations
of Cycles in this case because we are searching for the single
strongest detection, be it steady or flaring, and discarding the
remaining observations.  The
normalized probability is then calculated by selecting the
maximum TS (minimum probability) from this set, converting it
into a probability, and then normalizing this probability
for the number of trials using the equation:
\begin{equation}
P_{\rm peak}=1 - (1-p_{\rm min})^N
\end{equation}
where {\it N} is the number of cases examined, and $p_{\rm min}$
is the minimum probability in the set of observations.  This procedure,
refered to as the `Peak' method, excels at
finding sources that were detected strongly in a single
viewing period.  This is the preferred method for finding
blazars if the flaring timescale is comparable to a VP and
if they flare only once during the set of observations.  This
technique corresponds most closely to the standard 3EG analysis.

\subsubsection{Call for a 4EG Catalog}

Based on the {\it EGRET}\  analysis carried out in this work, we believe
that a fourth {\it EGRET}\  catalog is essential to preparation
for {\it GLAST}, due to reprocessing of the data since the
creation of the 3EG catalog.  In analyzing the current release of the {\it EGRET}\
data (assuming 3EG positions for the sources, but re-modeling the
fluxes and Test Statistics), we have found
several sources that would have been
dropped from the list after reanalysis.  One particularly
bad example is J1227+4302, whose peak detection drops down to
$\sqrt{\rm TS}=1.9$.
A dramatic decrease in photons in the vicinity of this source is
visible in comparing the current and 3EG {\it E} $>$ 100 MeV raw
count maps.
When comparing the distribution of TS values extracted from the
current {\it EGRET}\  data products (cossc.gsfc.nasa.gov - 'Current
Date' in the old and current maps are 27/8/96 and 27/3/01
respectively) to the 3EG
catalog, an overall drop in detection significance is apparent.
While the overall exposure in P1234 has increased in the current
reprocessing, the counts have decreased in both the $<$100 MeV
and $>$100 MeV maps.  More quantitatively, the counts decreased
by 2.3\% and 0.6\% in the $>$100 MeV and $<$100 MeV maps
respectively, while the exposure increased by 0.4\% and 0.3\%.
Additionally, improved Galactic foreground emission models may further
alter the extracted source list.

\section{Application of the Method}

\subsection{Low Significance 3EG Sources}

As a reality check, we compute the detection significance
by both methods for a subset of the 3EG detections.
In order to apply these methods to the 3EG sources,
we first have to generate TS maps from which
these sources are not excluded.  We create two sets
of these maps: one where 3EG sources with $\sigma>$ 4.75
are `cleaned' (modeled and removed), and one where $\sigma>$ 4.25
sources have been cleaned.
From these maps, we simply read off the TS values for each VP/Cycle at the
3EG positions of the $\sigma<$ 4.25 and $\sigma<$ 4.75 sources.  This
differs from the traditional {\it EGRET}\  method of modeling all sources
simultaneously (which we have also done).  Note that here the source
positions used were the 3EG $\gamma$-ray positions, not the positions
of radio counterparts, which should increase the apparent significance.
The distributions of Peak and Product probabilities for this sample are
plotted in Figure 2.

\clearpage
\begin{inlinefigure}
\figurenum{2}
\scalebox{1.0}{\rotatebox{0}{\plotone{f2.eps}}}
\figcaption{The probabilities are plotted for faint 3EG
sources for both the Product and Peak methods.  Pluses
and stars represent $4.25<\sqrt{\rm TS}<4.75$ and $\sqrt{\rm TS}
<4.25$ sources respectively.  The threshold for inclusion in the 3EG
catalog appears to be $\sim$2$\sigma$ after accounting for the
number of trials.
Both methods show a wide range of statistical significance, strongly
affected by the number of trials.  For the selected sources, this
dominates the range of the Peak method probability.
The two methods exhibit large differences in $\gamma$-ray
probabilities for individual sources and we believe these methods are
complementary.  The lowest significance point is J1227+4302, a
source whose peak TS dropped from $\sim$16 to $\sim$4 in the
current release of the data.}
\label{Fig2}
\end{inlinefigure}
\clearpage

Since we have correctly normalized for the number of trials, we expect
that the probabilities will be significantly lower than
the 3EG.  The significance threshold of sources in the 3EG catalog is
in fact closer to 2$\sigma$ when we account for the number of trials.
As noted above, in addition to the decrease in
significance due to the normalization process, we also find a
systematic drop in TS values for these sources in the current release
of the data, arguing that a fourth {\it EGRET}\  catalog should be created.

\subsection{The 3EG-Cleaned Background Distribution}

In order to determine whether the Peak and Product methods produce
reasonably normalized probabilities, we created a `background sample'
in the form of a grid of $0.5^\circ \times 0.5^\circ$ pixels spanning
$0^\circ<$decl.$<75^\circ$, $\vert b \vert > 10^\circ$ and a
minimum of $2^\circ$ away from modeled 3EG sources.  We then filled in
this grid with the actual TS values from the VP and Cycle maps.  Since we do
not model the `$3\sigma$ 3EG' sources or anything fainter, we
expect real sources to be present in this background.  However,
we anticipate that the low-TS values should be
distributed as true random background.  This is nearly the case
for the Product background distribution; however, the Peak
background distribution is far from random.  Therefore,
to compare these methods on equal footing, we must renormalize
these probabilities.

We choose to renormalize these probability
distributions by renormalizing the background probability distribution
to a uniform probability distribution.
This is accomplished by computing the occurrence-based
probability for survey sources from the background distribution.
That is, for a given Peak or Product probability, we total the number
of points in the respective background distribution with this
probability or lower, divide this by the total number of points
in the background, and assign this as our renormalized probability.
Because we know that this background includes numerous sources, all of
which span tens of pixels, this renormalization produces a very
conservative measure of the likelihood of $\gamma$-ray detection.
In effect, we are calculating the probability that a source is detected
more strongly than a random sky position, where the sky contains
unmodeled sources.

This procedure would not be necessary if there were no spatial
correlations in the data.  This is seen through the clustering
of TS = 0 detections seen at a significant fraction of positions
on the sky.  Of the 61,866 positions ($0.5^\circ \times 0.5^\circ$
pixels) that we consider in the north, we find that
more than 1000 positions have TS = 0 for every observation.  This is a
very significant excess over the $\sim$dozen such points we would
expect to find by chance.  We have confirmed via Monte Carlo that
combining an arbitrary number of uniformly distributed probabilities by
either the Peak or Product method results in a uniform distribution of
probabilities, demonstrating that these correlations do exist in the
data and are not intrinsic to the computation methods.

\subsection{Source Detection}

Now that the methods are well understood, we search the {\it EGRET}\  data
for the FoM-selected blazar candidates.
Each technique has its own merits, and we do not deem either method
superior.  Both the Peak and Product ranking methods
produce a significant detection of the blazar candidates above the
background.  The Peak method excels at finding sources that flare
up just once, especially when they sputter around below background
for the remainder of the observations.  By not including all
possible combinations of data -- we only include individual VPs, P1,
P2, P3, P4, P12, P34, and P1234 -- the Peak method misses sources
that exhibit multiple flares spanning several cycles (e.g., flaring in
P1 and P3).  Conversely, the Product
method is more efficient at finding sources that are detected multiple
times, especially sources where the largest TS is found in P1234.
The Product method is much more sensitive to the number of VPs in
which a position was observed.

\clearpage
\begin{inlinefigure}
\figurenum{3}
\scalebox{1.0}{\rotatebox{0}{\plotone{f3.eps}}}
\figcaption{Left: The cumulative distribution of probabilities for the
Peak method (dotted) and Product method (dashed) are compared to
the expected random distribution (solid).  Right: Scatter plot contrasting
the Peak and Product methods of calculating the $\gamma$-ray likelihood.
Sources detected with higher significance by the Product method appear above
the solid line and those detected more strongly by the Peak method lie below
this line.  Generally, most sources are best detected by the product method,
however a few flaring sources show up best as Peak method
detections at the bottom of the plot.}
\label{Fig3}
\end{inlinefigure}
\clearpage

As can be seen in Figure 3, both probability distributions deviate
significantly from a uniform random distribution.  We quantify this
significance in two ways.  First, we compare the distribution of
probabilities for the blazar candidates computed by each method to the
background distribution via the K-S test.  The resulting probabilities
are 0.00021 (3.7$\sigma$) and 0.0018 (3.1$\sigma$) for the Peak and
Product methods respectively.

Second, by setting several detection thresholds, we compile the number
of sources selected by each method.  These are shown in Table 3.
In Table 1, a sample page of the complete table, which is available
electronically, the Peak and Product probabilities are tabulated
for all sources that survive the spatial cuts.

\subsection{Does $\gamma$-ray Probability Correlate With FoM?}

Since we believe that the FoM is selecting {\it EGRET}-like blazars,
we expect a correlation between the FoM and the $\gamma$-ray
probabilities at a given location.
It is unclear whether blazars of comparable
radio brightness to the 3EG blazars are not strongly detected because
they were not actively flaring in $\gamma$-rays
during {\it EGRET}\  observations or because of a difference in the opening angle
of the radio and $\gamma$-ray beams.  Either of these effects
decreases the correlation between the FoM and the $\gamma$-ray
detection probability.  Of course, since these survey sources are
typically found to be very faint in $\gamma$-rays and background
fluctuations are comparable in magnitude, we do not expect to find a
strong correlation.

We examine the FoM/$\gamma$-ray probability correlation in the data
in three ways.  First,
for each probability scheme, we split the survey data by FoM into
two nearly equal parts (at FoM = 0.075) and compare the resulting
distributions to the background.  In the Peak case, both sets
show similar significance in departure from the background as
measured by the K-S test: FoM $>0.075 \rightarrow 0.034$, FoM $<0.075
\rightarrow 0.0095$.
However, for the Product method, the larger FoM set is much more
significant: FoM $>0.075 \rightarrow 0.0027$, FoM $<0.075 \rightarrow
0.28$.

Alternatively, we compute the Spearman rank correlation
for both the Peak and Product methods against the FoM.  The resulting
coefficients
(significances) are -0.07 (1.7$\sigma$) and -0.02 (0.54$\sigma$) for
the Product and
Peak methods respectively.  The correlation has the correct sign for
both methods since we expect the smaller probabilities for large FoMs.
For the Product method, the correlation is mildly significant; however,
for the Peak method, the results are insignificant.

Finally, we create a $\gamma$-ray selected subset of the survey by
selecting sources detected at the 95\% (2$\sigma$) level by either the
Peak or Product method and then examining the distributions of
corresponding FoM values.  Applying this cut, we find 41 sources by
the Product method (34 Peak), and the mean FoM value calculated for
these sources is 0.098 (0.089) compared to the average value of
0.083 for the whole survey.  Thus $\gamma$-ray selection appears
to select brighter, flatter radio sources than average, and the
Product method is more effective than the Peak method.  In all three
of the above tests, the strongest correlation is found between the FoM
and the Product method.

\section{Optical Follow-up}

Of our 710 survey blazar candidates, nearly half have archival
classification and assigned redshifts.  Information for these objects
was extracted primarily from the Eleventh Edition of the Quasar Catalog
(Veron-Cetty et al. 2003) and the Early through 3rd data releases of the
Sloan Digital
Sky Survey \citep{aba04}.  A handful of objects also appear in
the optically bright CLASS Blazar Survey \citep{cac02}, the only other
blazar survey drawn from CLASS sources.
As a follow-up, the remaining positions were
queried in the SIMBAD database.  The remaining objects are the
target of spectroscopic observations at McDonald Observatory.

\subsection{Hobby-Eberly Telescope/LRS Spectroscopy}

Spectroscopic observations were made using the Marcario Low
Resolution Spectrograph (LRS)
(Hill et al. 1998) on the 9.2 m Hobby-Eberly Telescope (HET)
(Ramsey et al. 1998).  These
targets were observed in regular queue operations from March 2002 to
October 2004.  Exposures ranged from 2 $\times$ 300 s to well over an hour
spanning several visits.  Image quality generally fell in the range of
1.5'' to 2.5''.  Observations employed a 300 lines mm$^{-1}$
grating and a 2'' slit for a dispersion of 4 \AA ~per (2$\times$2
binned) pixel and an effective resolution of 16 \AA ~covering
approximately $\lambda\lambda 4200-10000$.

Standard IRAF CCD reductions, calibrations, and optimal extraction were
performed.  Redshifts were derived whenever possible via cross-correlation
analysis with AGN and galactic templates using the IRAF RVSAO package.
Images of the extracted 1-D spectra are available online at
\url{astro.stanford.edu/northernblazars.html}.

We do not yet have spectroscopic data for 186 of the blazar
candidates and are still observing these objects with the HET.

\subsection{2.7 m/IGI Spectroscopy}

A handful of objects were observed with the 2.7 m Harlan J. Smith telescope
at McDonald Observatory.  Filler observations were made during an
observing run from 25-29 July 2003, primarily targeting
southern 3EG counterparts.  The Imaging Grism Instrument (IGI)
spectrograph (Gary Hill) was used with a 6000 \AA ~Grism and a 50 mm lens.
A 2'' slit was employed for the first 1.5 nights and a 2.5'' slit
thereafter due to generally poor imaging.  The imaging fluctuated around
1.5'' to 2'' on the best night, but typically held around 2'' to 2.5''.
The IGI setup covered a smaller wavelength range than the HET/LRS, namely
$\lambda\lambda 4250-8500$.  Due to a wide range of observing conditions
and source brightnesses, total exposures ranged from 300 to 3600 seconds.

\subsection{Classification}

As of this publication, we have obtained 167 new spectroscopic
identifications for objects selected by the FoM method.  The
redshifts and basic properties of these new blazar identifications
are listed in Table 1.  Sources observed with the HET or 2.7 m were
classified based on their observed
spectra, S/N permitting.  The observed sources fall into the following four
categories:  BL Lac objects, passive elliptical galaxies, flat spectrum radio
quasars, and narrow line radio galaxies.  The featureless spectra and
spectra with strong absorption lines were segregated into two categories:
BL Lac objects and passive elliptical galaxies.  BL Lac objects are
defined here by the following properties (Marcha et al. 1996): the break
contrast $ =(\frac{f^+ - f^-}{f^+}) < 0.4$, where $f^+$ and $f^-$ are the
fluxes
redward and blueward of the H/K break, and the rest-frame equivalent width
of the strongest emission line detected must be less than 5 \AA.  The
remainder of the absorption line objects
are classified as passive elliptical galaxies, although these appear to
have active nuclei.  For a handful of objects, only narrow emission lines
(kinematic width $<$ 1000 km/s) were observed and these were classified as
narrow line radio galaxies (NLRG).  All other emission
line objects were classified as flat spectrum radio quasars.

Archival data were classified based on the source classes
of the 11th
Veron-Cetty/Veron Quasar Catalogue, Sloan Digital Sky Survey and
SIMBAD queries.
Objects listed in the Veron catalog as Type 1-1.5 Seyfert galaxies,
active galactic nuclei and quasars were
classified as flat spectrum radio quasars. Seyfert Type 1.9 and above
were classified as narrow line radio galaxies.

\subsection{Survey Efficiency}

We find that the FoM method is extremely efficient at targeting blazars.
In the subset of the sample with reliable identifications, over 95\% of
sources are identified as FSRQs or BL Lacs.  Thus we find a factor of
3 fewer spurious sources by this method than in our
X-ray selected pilot survey.  Interestingly, $\sim$25\% of the
non-blazars found were X-ray detected, suggesting that requiring X-ray
detection for an AGN survey is more likely to select NLRGs and passive
ellipticals.

\subsection{Interesting Spectra}

This survey has produced several interesting objects.
The most noteworthy is J0906+6930, which we believe to be the highest
redshift blazar to date at {\it z} = 5.47 \citep{rom04}.  This is
also the highest redshift radio-selected object to date
and the brightest object at this redshift at 8.4 GHz.
Preliminary 2 cm VLBA snapshots find a jet-like
structure, providing more evidence for the blazar nature of this
object, and compact flux was also detected at 7 mm at the 40 mJy level.

One FSRQ, J1618+0819, exhibits extremely broad lines (FWHM$(v_{kin})>$ 17,000
km/s), where the Balmer lines are clearly multi-peaked, on top of a
very strong continuum.  J1855+3742, another FSRQ, shows a strong CII
line (2326 \AA) not generally observed in blazars, the
equivalent width of which is comparable to that of MgII.
Additionally, we find several new bright featureless BL Lac objects.
Spectra of these objects are shown in Figure 4.

\clearpage
\begin{inlinefigure}
\figurenum{4}
\scalebox{1.0}{\rotatebox{0}{\plotone{f4.eps}}}
\figcaption{Sample Spectra:
J0424+0805 -- A moderately high redshift FSRQ,
J1008+0621 -- A typical featureless BL Lac object,
J1719+1745 -- A source classified as BL Lac in the literature without
redshift - we have determined a robust redshift from our new
spectroscopy and confirm the BL Lac ID,
J0446+3900 and J1618+0819 -- FSRQs with extremely broad Balmer lines
(multiple components), and
J1855+3742 -- A weak-continuum FSRQ; note the unusual occurance of the
CII emission line.}
\label{Fig4}
\end{inlinefigure}
\clearpage

\section{Source Populations}

We can now compare this FoM-selected sample with the 3EG sample.  We believe
that this survey is composed of both a fainter extension of the 3EG as well
as sources that would have been detected by {\it EGRET}\  had they not been in a
low-flux state when observed.  We examine the redshift distribution and
source population of these samples as well as the effects of X-ray
selection.

\subsection{Redshift Distribution}

The primary difference between sources in this sample and the 3EG
counterparts is simply the proximity to strong {\it EGRET}\  $\gamma$-ray
detections.  The redshift distributions of these two samples are
indistinguishable by the K-S test (Prob$_{\rm K-S}=0.19$).  For
comparison, the redshift histogram of FSRQs from this work
is plotted against the distribution of 3EG counterparts (SRM03, SRM04)
in Figure 5.
Only the FSRQs are considered in this exercise since for the BL Lacs we
have a much smaller number of redshifts, and the redshift measurements are
much less uniform than in the well observed 3EG sample.
The X-ray detected survey sources are on average less distant
than the non-X-ray detected sources.  The mean redshifts of the FoM
survey blazar candidates are 1.08 and 1.52 for the X-ray detected and the
non-X-ray detected sources respectively, averaging to 1.37 overall.
Our DXRBS-like survey, which required X-ray detections, had an even lower mean
redshift of 0.84.  The 3EG blazar
counterparts fall at a slightly lower redshift of {\it z} = 1.32 on average but
are consistent with the FoM-selected distribution.
Not surprisingly, requiring X-ray detections selects a more local
population of sources since the RASS is a relatively shallow survey.
The set of blazar candidates detected in the RASS were on average 50\%
brighter at 8.4 GHz than those not seen in X-rays.  Additionally, the
X-ray detected FoM-selected blazar candidates are 1.3 magnitudes (USNO
B1.0 R2 magnitude)(Monet et al. 2003) brighter optically than the rest.
These tend to be
`high peak' blazars (HBL) with the synchrotron peak extending to the
optical and X-ray \cite{up95}.  These will be relatively low luminosity
$\gamma$-ray sources.

\clearpage
\begin{inlinefigure}
\figurenum{5}
\scalebox{1.0}{\rotatebox{0}{\plotone{f5.eps}}}
\figcaption{Redshift histograms of the 3EG FSRQs (filled)
and the survey FSRQs (dotted line).  Comparing the two
distributions via the K-S test results in a probability of
0.19 that they are drawn from the same parent distribution.}
\label{Fig5}
\end{inlinefigure}
\clearpage

\subsection{BL Lac Fraction}

In the 3EG sample, above decl. = -40$^\circ$ and away from the Galaxy, we found
$\sim$18\% BL Lac objects and $\sim$78\% flat spectrum radio quasars.
To date, in the FoM-selected survey we find a lower BL Lac fraction
of $\sim$13.6\%.  This likely stems from the fact that the 3EG
sample is nearly complete, while the FoM sample only has identifications
for $\sim$74\% of the sources, where the majority of these IDs are archival.
Clearly FSRQs, which generally have very strong emission lines, require
lower S/N to make a solid ID and thus are more likely to be identified
than BL Lacs.

In the original X-ray selected sample, we found 39\% of the objects
to be BL Lacs, along with a significantly lower efficiency for finding
blazars (86\%).  In the FoM-selected set, we have classifications for 30
BL Lacs and 143 FSRQs (17.3\% BL Lacs) detected in X-rays.
The BL Lac
fraction is much smaller for sources not detected in the RASS:
we find 38 BL Lacs and 288 FSRQs (11.7\% BL Lacs).  Thus,
as expected the
X-ray detection criteria select a significantly larger percentage of
BL Lac objects.

\section{Conclusions}

We have compiled a survey of 710 objects selected from radio and X-ray
data to have properties similar to the 3EG blazar counterparts.
Of these objects, we have contributed 167 new spectroscopic
identifications along with robust redshifts for the majority.
Our spectroscopy represents an improvement of $\sim$50\% over the
archival IDs in the northern sky.  Because these sources
were selected in the same way as the 3EG counterparts but were not
detected in the 3EG catalog, we believe that many of these sources
were simply in low states during their {\it EGRET}\  exposures.  However, we
cannot rule out the possibility that the differences in the $\gamma$-ray
and radio beaming may preclude detections of these sources in the GeV
range.
We introduce two means of statistically ranking {\it EGRET}\  $\gamma$-ray
detections by combining information collected during the
survey phase of the mission.  Providing further evidence for the
blazar nature of these sources, we have convincingly detected
the signal of these FoM-selected candidate blazars in the
{\it EGRET}\  data at the $\sim$3.5$\sigma$ level by both of these
methods.  However, the FoM for individual sources was only
weakly correlated with the significance of excess $\gamma$-ray flux.

{\it GLAST}\  will help test whether these
FoM-selected sources are strong $\gamma$-ray emitters.  In
addition, we expect that {\it GLAST}\  will put tighter constraints on
the typical duty cycle of blazars.  Based on the findings
in this work, we also believe that a 4EG catalog needs to be created
to adequately model the blazar population in preparation
for {\it GLAST}.  Since {\it GLAST}\  will of course produce an all-sky survey, we
are extending a CLASS-like VLA survey south of decl. = 0$^\circ$ from
which we expect to draw a similar number of $\gamma$-ray blazar
candidates.  Ultimately we seek to identify a nearly uniform all-sky
set of 2,000-3,000 blazars to match the expected {\it GLAST}\  detections.

\acknowledgments

DSE and SEH were supported by SLAC under DOE contract DE-AC03-76SF00515, and
PFM acknowledges support from NASA contract NAS5-00147.

redpajama_set_name: RedPajamaArXiv


text:
mkdir -p "$PREFIX/bin"
export MACHTYPE=x86_64
export BINDIR=$(pwd)/bin
export L="${LDFLAGS}"
mkdir -p "$BINDIR"
(cd kent/src/lib && make)
(cd kent/src/htslib && make)
(cd kent/src/jkOwnLib && make)
(cd kent/src/hg/lib && make)
(cd kent/src/utils/bigWigInfo && make)
cp bin/bigWigInfo "$PREFIX/bin"
chmod +x "$PREFIX/bin/bigWigInfo"


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text:
Pakistan beaten by Morgan-inspired England in lone T20
Home skipper hits unbeaten 57 as hosts win by 7 wickets
Published: May 06, 2019 02:30 AFP
England's Eoin Morgan and Joe Denly celebrate their win against Pakistan. Image Credit: AP
Cardiff: England captain Eoin Morgan led his side to a seven-wicket win over Pakistan in a lone Twenty20 international in Cardiff on Sunday with an unbeaten innings of 57.
Test skipper Joe Root made 47 and James Vince 36 as England overhauled Pakistan's total of 173 for six with four balls to spare at Sophia Gardens.
It was England's second victory in three days after their one-day international success away to Morgan's native Ireland in Dublin on Friday as they continued an encouraging start to a season that sees them staging both the 50-over World Cup and the Ashes.
England fast bowler Jofra Archer also continued his push for a World Cup call-up by taking two for 29.
"Jofra came on from the game in Ireland, he showed a lot more what he's about," said Morgan. "It's another debut and they don't always go well. The majority of the time they don't.
"He and the other bowlers will have the opportunity to show what they can do (in the one-day series against Pakistan)."
"But it's been a while, before the Ireland game, that he's played 50-over cricket, and we're conscious of not over-bowling him," he added.
Vince's attractive innings ended when he was caught down the legside by Pakistan captain and wicket-keeper Sarfraz Ahmed off Imad Wasim, but Morgan kept the runs coming, taking 14 off three successive balls from medium-pacer Faheem Ashraf.
And even when Sarfraz caught Root, there was little danger to England's hopes of victory, with Morgan hitting five fours and three sixes in his 29-ball stay.
Earlier, There was a bizarre incident at when the ground gave way beneath England's David Willey as the seamer was just about to make his delivery stride.
Fortunately for England, Willey avoided serious injury.
Babar Azam (65) and Haris Sohail (50) shared a stand of 103 after Pakistan had been 31 for two following Sarfraz's decision to bat first on a green-tinged pitch.
Haris hit Chris Jordan for six and Babar struck successive sixes off spinner Joe Denly before completing a 31-ball fifty.
Pakistan then saw both their well-set batsmen fall in quick succession with Barbados-born Archer, renowned for his form in T20 franchise cricket, removing Haris before he ran out Babar.
"We were about 10-12 runs short," said Sarfraz, ahead of Wednesday's ODI opener at The Oval. "Eoin Morgan and Joe Root batted well and we were always struggling after that."
More From Cricket
No 500 total, big hits still decide World Cup champion
Rohit, Bumrah in ICC's World Cup XI, no place for Kohli


text:
Il Campionato Primavera 1998-1999 è stata la 37ª edizione del Campionato Primavera.
La squadra vincitrice del torneo è stata l'Empoli, che si è aggiudicata il titolo di campione nazionale per la prima volta nella sua storia.

Prima fase

Girone A

Legenda:
      Ammessa alla seconda fase.

Note:
Tre punti a vittoria, uno a pareggio, zero a sconfitta.

Girone B

Legenda:
      Ammessa alla seconda fase.

Note:
Tre punti a vittoria, uno a pareggio, zero a sconfitta.

Girone C

Legenda:
      Ammessa alla seconda fase.

Note:
Tre punti a vittoria, uno a pareggio, zero a sconfitta.

Girone D

Legenda:
      Ammessa alla seconda fase.

Note:
Tre punti a vittoria, uno a pareggio, zero a sconfitta.

Seconda fase

Girone A

Legenda:
      Ammessa alla fase finale.

Note:
Tre punti a vittoria, uno a pareggio, zero a sconfitta.

Girone B

Legenda:
      Ammessa alla fase finale.

Note:
Tre punti a vittoria, uno a pareggio, zero a sconfitta.

Girone C

Legenda:
      Ammessa alla fase finale.

Note:
Tre punti a vittoria, uno a pareggio, zero a sconfitta.

Girone D

Legenda:
      Ammessa alla fase finale.

Note:
Tre punti a vittoria, uno a pareggio, zero a sconfitta.

Fase finale

Quarti di finale
Disputati il 28 e 29 maggio 1999

Semifinali
Disputati il 31 maggio e 1 giugno 1999

Finale
Disputata il 4 giugno 1999 a Lignano Sabbiadoro

Bibliografia
 Carlo Fontanelli, Annogol 2000, GEO Edizioni.

Calcio nel 1998
Calcio nel 1999
1998

redpajama_set_name: RedPajamaWikipedia


text:
Robbie Coltrane's daughter shares picture of them together as Harry Potter co-stars pay tribute
By Jhon Lobo On Oct 15, 2022
Robbie Coltrane's daughter has shared a touching picture of the pair together, following his death aged 72.
Alice McMillan posted the photo of her hugging her father on Instagram on Saturday, accompanied by a black heart emoji.
Coltrane is survived by Alice and her brother Spencer, their mother Rhonda Gemmell and his sister Annie Rae.
The actor and comedian's agent of 40 years announced his death on Friday.
She did not give details of how he died, but Coltrane's family thanked staff at Forth Valley Royal Hospital in Larbert, Scotland, for their care.
Coltrane, best known for playing Rubeus Hagrid in the Harry Potter films, also played criminal psychologist Dr Eddie 'Fitz' Fitzgerald in the 1990s crime drama Cracker.
Pic: Lux/The Hollywood Archive/Alamy
It won him the best actor prize at the British Academy Television Awards three years running, before he was made an OBE in 2006.
News of his death sparked tributes from several of his Harry Potter co-stars.
Author of the books JK Rowling said: "I'll never know anyone remotely like Robbie again. He was an incredible talent, a complete one off."
Emma Watson, who played Hermione Granger in the films, shared an image of the pair of them, describing him as "like the most fun uncle I've ever had".
"Robbie, if I ever get to be so kind as you were to me on a film set I promise I'll do it in your name and memory," she wrote.
"There was no better Hagrid. You made it a joy to be Hermione."
Daniel Radcliffe, who starred as Harry Potter, said: "Robbie was one of the funniest people I've met and used to keep us laughing constantly as kids on the set.
"I've especially fond memories of him keeping our spirits up on Prisoner of Azkaban, when we were all hiding from the torrential rain for hours in Hagrid's hut and he was telling stories and cracking jokes to keep morale up."
While James Phelps, who played Fred Weasley, said he will miss the "random chats about all subjects under the sun".
Tom Felton, who played Draco Malfoy, described Coltrane as a "big friendly giant", and recalled shooting a scene with him during Harry Potter And The Philosopher's Stone.
"One of my fondest memories of filming Harry Potter was a night shoot on the first film in the forbidden forest," Felton tweeted.
"I was 12. Robbie cared & looked after everyone around of him. Effortlessly. And made them laugh. Effortlessly. Love you mate – thank you for everything xx."
Matthew Lewis, who played Neville Longbottom, described Coltrane as "a giant, in more ways than one" and said they "shared a love of the final frontier".
Bonnie Wright, who featured as Ginny Weasley, said she was "heartbroken" and thanked Coltrane for "all the laughter".
'Such a sweet man – such depth, power and talent'
Sir Lenny Henry, who voiced Dre Head in Harry Potter And The Prisoner Of Azkaban, tweeted: "This is awful news. Rob was the real thing. Condolences to his family. Big love big fella xxx"
Stephen Fry, who voiced the Harry Potter audio books, said Coltrane would be "dreadfully missed".
He said he met Coltrane almost 40 years ago, adding: "Such depth, power & talent: funny enough to cause helpless hiccups & honking as we made our first TV show, Alfresco."
Hugh Laurie, who also acted alongside Coltrane in Alfresco, and the period sitcom Blackadder, recalled fond memories of his time with the actor.
Fellow Blackadder star Tony Robinson described him as "such a sweet man" and "so talented as a comic and as a straight actor".
He added in a post to Twitter: "'Dictionary' was my favourite episode of the Adder ever and it was all down to you mate. Rest well x"
Actor Robert Lindsay, who starred alongside Coltrane in the 1989 film Bert Rigby, You're a Fool paid tribute to his "dear pal", adding: "We shared a Hollywood journey that will live with me forever."
Scotland's First Minister Nicola Sturgeon has called Coltrane a "Scottish entertainment legend" and said he will be "hugely missed".
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text:
Dennis Evicted From Big Brother
Housemate Dennis McHugh has been removed from the Big Brother house for unacceptable behaviour
Friday, June 27, 2008 - 14:39
Big Brother's Dennis was removed from the house for unacceptable behaviour earlier today.
A number of housemates were involved in an argument at approximately 12.45am this morning (27th June), which resulted from a prank played by Rex that ended in a picture painted by Jennifer being slightly defaced.
During the argument Dennis spat in the face of fellow housemate, Mohamed.
Big Brother intervened immediately to break up the argument. The 'as live' streaming from the house on E4 was cut and no footage was broadcast.
Dennis was called to the diary room a second time at 1:15pm and told he was immediately being removed from the house.
A Channel 4 spokeswoman said: "Spitting in someone's face is seriously offensive and Mohamed was understandably upset.
Dennis is the second Big Brother housemate to be removed from the house.
Alex was removed for repeated unacceptable behaviour last week.


text:
Q: Calculating determinant from LUDecomposition As far as i know LU decomposition allow you to calculate matrix determinant following easy and cheap formula: Det[A] = Det[L] Det[U] = Det[U]
Trying this out in Mathematica 7 gives me correct result by absolute value, i.e. it ignores negative determinants and transforms them to positive ones.
Sample code:
matrixA = {{-1, 2, 3, 5}, {-7, -4, 5, 4}, {-89, 7, 8, -6}, {8, 6, -1, 4}};

Det[matrixA] gives out -2067
but
{lu, p, c} = LUDecomposition[matrixA]

u = lu SparseArray[{i_, j_} /; j >= i -> 1, {4, 4}]

Det[u] is 2067
Well, the question is obvious - how to get correct determinant in Mathematica using LU decomposition?

A: Well, this is because you forgot to take into account the permutation matrix that is output by the LU decomposition routine. You have to remember two facts: 1.) Gaussian elimination generally performs row interchanges for numerical stability reasons, and 2.) the determinant of a matrix changes sign if you interchange rows.
In Mathematica at least, the function that will rescue you is Signature[], which gives the signature of the permutation required to turn the permutation matrix (which Mathematica outputs as a scrambled list of the numbers from 1 to n, where n is the size of your matrix) into the identity matrix.
So, to use your example in Mathematica:
m={{-1, 2, 3, 5}, {-7, -4, 5, 4}, {-89, 7, 8, -6}, {8, 6, -1, 4}};

we compare
Det[m]
-2067

with the following:
{lu, p, c} = LUDecomposition[m]
{{{-1, 2, 3, 5}, {7, -18, -16, -31}, {-8, -11/9, 31/9, 55/9}, {89, 19/2, -963/31, 2067/62}}, {1, 2, 4, 3}, 1}

Now, LUDecomposition[] here outputs three things: the merged $\mathbf{L}$ and $\mathbf{U}$ matrices, the permutation, and the condition number. We can get the tentative determinant by multiplying together the diagonal elements of lu, thus:
Tr[lu, Times]
2067

Here is where Signature comes in:
Signature[{1, 2, 4, 3}]
-1

Note that to turn {1, 2, 4, 3} into {1, 2, 3, 4}, one needs one swap; namely, to swap the third and fourth elements. Since 1 is odd, the signature is -1.
Thus,
Signature[p]*Tr[lu, Times]
-2067

gives the correct answer.

A: From the documentation: "Therefore multiplying L and U recreates the original matrix permuted with the row pivot vector." So you need to multiply by Signature[p] to get the correct sign.

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