Florida reels from Orlando massacre.
TALLAHASSEE, Fla. - Terrorism hit home this week.
Floridians woke up Sunday morning to the unthinkable. On Saturday night, young people crowded into an Orlando club for music, dancing and the simple joys of being with friends. Hours later, 49 clubgoers were dead and dozens more were wounded.
Mayor Buddy Dyer described Sunday as "probably the most difficult day in the history of Orlando." For lesbian, gay, bisexual and transgender Floridians, it carried the extra weight of knowing that a gay club had been targeted.
Orlando police were hailed as heroes for going into the Pulse nightclub and ultimately killing the shooter, who claimed to support the Islamic State terrorist group. State, federal and local officials also converged during the week to lend support to the family members of victims.
Florida, however, won't ever be the same. Omar Mateen was a virtual nobody from St. Lucie County. But he was able to carry out the worst mass shooting in U.S. history --- and make Floridians feel vulnerable.
Gov. Rick Scott, Attorney General Pam Bondi and U.S. Sens Bill Nelson and Marco Rubio quickly joined authorities Sunday in Orlando to try to sort out what had happened and to help oversee assistance for the reeling community.
"Clearly, this is an act of terrorism. You just can't imagine this happening in any community," Scott said. "My heart goes out to every family member that's been impacted. … This state is going to be defined as a state of generosity, a state of love. We are a resilient state. We love people in our state and we are going to continue to do that."
Rubio, R-Fla., said Sunday that the attack "could happen anywhere in the world."
"Unfortunately, today was Orlando's turn," he said. "We know that there's hate in the world. We know that some of it is inspired by warped ideology. … I hope they see today they won't terrorize America. They won't terrorize Floridians. We stand with all Americans … irrespective of their sexual orientation."
While Rubio raised the issue of sexual orientation, some gay activists said in the days after the attack that they thought the LGBT community was being ignored.
"I think it's pretty much gone viral that our political leaders not only in Florida but throughout the country need to say the words that this was an attack on our gay community," said Christian Ulvert, a Florida Democratic political consultant who is gay. "You have to say those words."
Speaking to reporters at the White House on Sunday, Obama called the massacre "an act of terror and an act of hate" that was "especially heartbreaking for all of our friends … who are lesbian, gay, bisexual or transgender."
On Thursday, Obama and Vice President Joe Biden traveled to Orlando to comfort the family members of victims and survivors.
"Their grief is beyond description," Obama said after he and Biden spent two hours at the Amway Center, meeting privately with people who lost loved ones in the attack. "These families could be our families. In fact, they are our family. … And today the vice president and I told them, on behalf of the American people, that our hearts are broken, too."
Debates about gun rights and gun control never go away. But after a tragedy like the Orlando killings, the debates get ratcheted up.
Mateen, a security guard, passed all of the legally required background checks for his weapons.
"He held a 'D' license, as well as a 'G' license, which means that he is a security guard and a security guard who is permitted to carry a firearm," state Agriculture Commission Adam Putnam, whose agency oversees weapon permits in Florida, told reporters on Monday.
"All of the information related to his application to receive those licenses was in order," Putnam added. "He was fingerprinted. He successfully completed the application, had a criminal background check. There is nothing in that record that would have disqualified this individual, who was a U.S. citizen, who had a clean criminal record, who underwent a background check and mental-health screening."
That doesn't mean, however, the debates will go away. Democratic lawmakers held a news conference Wednesday in Orlando and called for a special legislative session to address gun-control measures.
"I don't think there is anyone here who opposes a person's right to defend themselves," Sen. Geraldine Thompson, D-Orlando, said. "But what do you need for self-defense? Do you need a bazooka? Do you need a flame thrower? Do you need a rocket launcher? Do you need an assault-style weapon? It is those kinds of things we want to examine in the special session."
Republican legislative leaders, however, said they didn't see a need for a special session. Marion Hammer, the longtime Tallahassee lobbyist for the National Rifle Association and the Unified Sportsmen of Florida, said in an email that the special session request by "these ultraliberal, gun hating Democrats" is "political grandstanding."
"They are attempting to exploit a tragedy for political gain," Hammer said in the email.
Meanwhile, GOP political consultant Rick Wilson gave a bottom-line analysis of why the terrorist attack will not spur the Republican-dominated Legislature to pass gun-control measures.
"Democrats say this is all about gun control, and Republicans say this is all about Muslims. Now, the important thing to remember is that our society has largely made up its mind on guns. A tragedy like this, just speaking in cold political terms, doesn't move the needle," he said. "If people look at this as a competition between security versus gun control, security wins every time."
Quickly after the shootings, elected officials and political candidates started flooding social media and inboxes with messages about issues such as gun control and cracking down on terrorists.
But with the November elections less than five months away, the political ramifications of the shootings remained somewhat murky this week.
Wilson, for example, suggested that the attack might have little impact on the elections.
"As horrifying as this is, as terrible as this is, human grief has sort of a span of time where it affects people," he said. "It doesn't diminish the horror of this thing to note that, as a country, we have a short attention span. We always have."
But others said anger and grief about the massacre won't go away before the Aug. 30 primary elections or the November elections. Some said the mass murder certainly won't fade away for LGBT people or Hispanics, who made up many of the victims at the club.
"It's going to be a wake-up call," said Carlos Guillermo Smith, a state House candidate who is governmental affairs director for the advocacy group Equality Florida.
Probably the most tangible political result this week was that Rubio, in light of the tragedy, indicated he might be reconsidering his decision not to seek re-election.
"Obviously, I take very seriously everything that's going on --- not just Orlando, but in our country," Rubio told reporters, according to The Hill, a Washington-based publication. "I enjoy my service here a lot. So I'll go home later this week, and I'll have some time with my family, and then if there's been a change in our status I'll be sure to let everyone know."
But Lt. Gov. Carlos Lopez-Cantera, a longtime Rubio friend who has been running for the Senate seat, said he would step aside if Rubio wants to get into the race.
"As friends for 20 years, this race is so much bigger than the two of us, and, as you have heard me say on the trail, this race isn't about an individual, this race is about Florida and the future of our country," Lopez-Cantera said in an email to supporters Wednesday. "I am still in this race and nothing has changed. However, if Marco decides to enter this race, I will not be filing the paperwork to run for the U.S. Senate."


I haven't taken the time to blog about politics lately, not only because I've been so busy, but also because nothing has moved me enough to take the time to sit down and move anything beyond a quick draft post. What happened this week was different.
I cannot make sense of the controversy surrounding Ted Koppel's reading of our fallen heros' names on Nightline. Before I go on I must admit that I wasn't able to watch the show last night so I can't speak to how it was presented.
It is no secret that I strongly support Operation Iraqi Freedom and that I don't want to see an early withdrawal or anything that would leave Iraq half finished. I feel our troops are making great progress and having lots of success battling the evil there; instead of here.
Whats the harm in tributing those who have gave their lives for this? I've had this link, on the right, on the front page of this site since I started this blog. Anyone who has made this great scrafice deserves nothing less than to be remembered for what they did. We should all memorize their names, think of them and their scrafice, and pray for those that they left behind.
But in a larger sense, we can not dedicate -- we can not consecrate -- we can not hallow -- this ground. The brave men, living and dead, who struggled here, have consecrated it, far above our poor power to add or detract. The world will little note, nor long remember, what we say here, but it can never forget what they did here. It is for us the living, rather, to be dedicated here to the unfinished work which they who fought here have thus far so nobly advanced. It is rather for us to be here dedicated to the great task remaining before us -- that from these honored dead we may take increased devotion to that cause for which they gave the last full measure of devotion -- that we here highly resolve that these dead shall not have died in vain -- that this nation, under God, shall have a new birth of freedom -- and that government of the people, by the people, for the people, shall not perish from the earth.
"But we felt that the impact would actually be greater on a day when the entire nation is not focused on war dead," he said.
That, and the fact that he's doing it during sweeps.
Look, it is a good thing, but when the motivation is obviously ratings and shock value, I'd prefer Koppel not use troops who sacrificed as a prop.


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Under Florida probate law, is there a statute of limitations for a claim against the decedent or the decedent's estate?
On Behalf of Lins Law Group, P.A. | Jun 2, 2014 | Probate |
In addition to the time frame set forth in Florida's non-claim statute (contained in Section 733.702 of Florida Statutes), the Florida Probate Code establishes a two-year statute of limitations for asserting claims against the decedent and the decedent's probate estate.
Section 733.710 sets forth this limitation period by providing that neither the decedent's estate, the personal representative, nor the beneficiaries shall be liable for any claim or cause of action against the decedent if not brought within two years of the decedent's death. This limitation period applies regardless of whether letters of administration have been issued and regardless of whether a probate has been opened.
Being aware of this two-year period is important because its consequences can be different than an applicable statute of limitation if the person had not died. For example, consider a situation where Party A and Party B enter into a written contract, after which time Party A breaches the contract. If Party A then dies, Party B must assert his claim for breach of contract within the earlier of two years from Party A's death or four years from the date of breach (the limitation period for breach of a written contract is four years in Florida).
One exception to this two-year limitation period applies a creditor who has filed a claim within two years after the person's death, and whose claim has not been paid or otherwise disposed. For this reason, when a creditor has a claim against a deceased person, the creditor would be well-served to consult a lawyer and to file a claim even if no probate is pending. This can be done under applicable Florida law, even if there is no probate filed, by filing the creditor's claim with the Clerk of the Circuit Court in the county where the decedent resided at the time of death.
As with the non-claim statutes, another exception to the two-year limitation period applies where there is a duly recorded mortgage or security interest or the lien of any person in possession of personal property or the right to foreclose and enforce the mortgage or lien.

redpajama_set_name: RedPajamaCommonCrawl


text:
'We are one race'
Published 8:20 pm Tuesday, June 2, 2020
A Justice for George Floyd Rally was held Tuesday evening diagonally across from the Freeborn County law enforcement center. Floyd died last week while in Minneapolis Police Department custody, igniting rallies, protests and demonstrations across the state, country and the world. - Colleen Harrison/Albert Lea Tribune
Members of the Albert Lea Police Department, including Public Safety Director JD Carlson, left, kneel during Tuesday's Justice for George Floyd Rally in Albert Lea. - Colleen Harrison/Albert Lea Tribune
Other names and instances of Black people who died while in police custody were read off during Tuesday's rally. - Colleen Harrison/Albert Lea Tribune
Some of the rally's attendees walked through downtown Albert Lea on Tuesday after the threat of severe weather rolling in partially broke up the rally. - Colleen Harrison/Albert Lea Tribune
Those who were able to were asked to kneel Tuesday during a moment of silence for George Floyd at an Albert Lea rally asking for justice for his death. - Colleen Harrison/Albert Lea Tribune
A viral video of George Floyd, a black man who died in police custody after he was in handcuffs when a white Minneapolis police officer pressed his knee into his neck as he pleaded that he couldn't breathe, has led to calls for justice around the world. - Colleen Harrison/Albert Lea Tribune
Thomas Martinez speaks during Tuesday's Justice for George Floyd Rally while rally organizer Hannah Goodemann looks on. - Colleen Harrison/Albert Lea Tribune
People were welcome to take turns coming up and speaking during the rally in honor of George Floyd. - Colleen Harrison/Albert Lea Tribune
Members of the Albert Lea Police Department helped pass out water bottles during Tuesday's rally as humidity helped send the heat index close to 100 degrees. - Colleen Harrison/Albert Lea Tribune
Day Peace speaks during Tuesday's rally for George Floyd. - Colleen Harrison/Albert Lea Tribune
Albert Lea Public Safety Director JD Carlson speaks during the Justice for George Floyd Rally. - Colleen Harrison/Albert Lea Tribune
Members of the Albert Lea Police Department kneel along with others attending Tuesday's Justice for George Floyd Rally in Albert Lea. - Colleen Harrison/Albert Lea Tribune
Those attending Tuesday's rally raise their fists in the air during a moment of silence for George Floyd. - Colleen Harrison/Albert Lea Tribune
Those in attendance chant different sayings led throughout Tuesday's rally. - Colleen Harrison/Albert Lea Tribune
A Justice for George Floyd Rally was held Tuesday evening diagonally across from the Freeborn County law enforcement center. - Colleen Harrison/Albert Lea Tribune
Some Justice for George Floyd rally attendees walk through downtown Albert Lea on Tuesday. - Colleen Harrison/Albert Lea Tribune
Rally held in honor of George Floyd asks for justice, change
Eight days after the death of George Floyd in Minneapolis, a few hundred people gathered in Albert Lea north of the Freeborn County Courthouse Tuesday to protest against Floyd's death and to open a dialogue for change.
Floyd, 46, was arrested for allegedly using a counterfeit $20 bill to pay for goods at a grocery store and died after a white officer pressed his knee into Floyd's neck for minutes, even after he stopped moving. That officer has been charged with third-degree murder in the case, and officials continue to investigate the other three who were also at the scene.
Twenty-one-year-old rally organizer Hannah Goodemann, who was born and raised in Albert Lea, said she felt that remaining silent in a time like this was unacceptable. She said though talking about racial issues makes people uncomfortable, she thought it was important to demand justice for his family.
"I hope tonight we can peacefully, but loudly, make our voices heard," Goodemann said.
Attendees of the rally gathered in the county parking lot at the intersection of Newton Avenue and College Street, and organizers encouraged people to practice social distancing and wear face masks. With high temperatures and humidity, Albert Lea police officers handed out water to attendees.
"George Floyd's life mattered," Goodemann said.
Other names and instances of other Black people who died while in police custody or in racial shootings were also read off at the event.
Many talked about the need for change on a greater scale but also credited the Albert Lea Police Department for its work in the community.
Albert Lea Public Safety Director J.D. Carlson said no one in law enforcement condones what happened to Floyd and said though he is proud to be a Minnesotan and noted that Minnesota police are highly trained, he knows they can always be better. He invited people in the crowd to remember the Albert Lea Police Department has an open door policy and that if anyone needs anything, they can always reach out or ask him.
Two people who grew up in the Civil Rights movement talked about how they advocated for change decades ago, but sadly many of the same things are still happening today.
Another person who spoke at the rally said a few years ago he stayed inside his home because he was scared of going outside and having people see his skin color. He tried to stay in his room with his blinds shut tight, hoping in some way he could lighten his skin color so people would like him more.
"We should not be afraid to go outside," he said, noting he still has social anxiety. "We should not be afraid of getting pulled over. We should not be afraid of going to school and getting bullied. We should be afraid of going to the store. We should not be afraid of walking outside with the risk of being shot or killed because someone does not like the way we look."
Day Peace, a comedian who lives in Lake Mills and is originally from Detroit, said he felt a sense of belonging attending the rally with his 7-year-old son Drake.
"Peaceful protest is powerful," Peace said.
He noted he attended his first protest while living in Phoenix in 2016, following the death of Alton Sterling, a black man killed by a white police officer in Baton Rouge, Louisiana. The trial has been pushed back for several reasons the last two years.
"I don't think it's too early to share what's going on," he said about his son.
Desiree Talamantes of Albert Lea said she decided to attend the rally because she felt it was time to speak out and speak up with the movement.
"I have three mixed daughters, and I don't want them to grow up in this world," she said.
She carried a sign that said, "We're not trying to start a race war. We're trying to end one."
"We all should be equal," she said. "We are one race — the human race."
She said she believes and hopes change will happen.
Melanie Gooden, who lives in Iowa but works in Albert Lea, attended the event with her husband, John Szymanowski, and daughter, Samantha Szymanowski.
"What happened is horrible," Gooden said. "It's time for this to stop."
She said her daughter wanted to come to a protest, and they thought it would be a good experience for her. She noted they were pleased with the turnout and that it stayed peaceful.
As the clouds darkened and the formal event ended, many in the crowd began walking through the downtown streets, carrying their signs and chanting to remember Floyd and that "Black lives matter."
Heavy winds and heavy rain sent most of the participants in separate directions before 6:30 p.m.
Many gather to recognize Veterans Day
United South Central presents "The Lion King Jr."
Albert Lea High School to perform "Mamma Mia!"
Gallery: Albert lea girls' hockey begins practice after historic run last year


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A 'reverse mortgage' is a new way of borrowing money for people 60 or older and own a home or condo to qualify for a reverse mortgage in Canada. The flexibility of never having to make monthly payments is why reverse mortgages are such an attractive option for thousands of Canadian homeowners.
Some people love them while others say they're a dangerous last resort.
A Canadian reverse mortgage allows people who are house-rich and cash-poor – many of whom could be seniors on pensions, who have their home paid off and are over 60 – to receive the option of receiving all the money you're eligible for in one lump sum advance, or you can take some now and more later, or you can receive planned advances over a set period of time. You can even combine a lump sum advance at the beginning with ongoing advances over time.
For most of these seniors, their home is their largest asset, yet they can't borrow against it because they cannot afford a monthly payment against the balance.
A reverse mortgage works differently. You can make monthly interest payments if you want to, but most people choose to pay back the mortgage when they sell their home.
Pay off a current mortgage - No More Payments!!!
As long as you're alive and haven't sold your house, you don't make any payments on the money you borrow.
But once you sell the house or die, the principal and accumulated interest must be paid back from the profits on the sale of the house.
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Today, we continued to read Persepolis, focusing on "The Letter", "The Party", and "The Heroes". Students began to look at elements of the coming of age story and how, Marjane's childhood can relate to our own lives.
There is no homework for tonight. However, I have posted extra credit questions for the chapters we have read. This is due April 28, 2016. No late work will be accepted for this.
If you missed class, be sure to look on line for the chapters (the page can be found under the more section). Read and annotate the chapters. Be sure to follow our annotation format.
If you have missed the vocab quiz, be sure to take it by Friday. It is your responsibility to come in to class, before school, at lunch or after school.


As the festive season draws ever closer, many of us find ourselves helping our little ones write their letters to Santa with a never-ending list of the latest toys, gizmos and gadgets that they want to wake up to on Christmas morning. It's easy to forget how lucky we are in comparison to other people living in absolute poverty.
People like the 60 million people in rural India living without access to safe, clean water to drink, cook and clean with. As a mother myself who spent her early parenting days endlessly sterilising bottles, dummies, rattles etc I can't imagine the anguish mothers in rural India must feel knowing that their only option is to allow their precious children to drink unsafe water. Water that accounts for 21% of all diseases and deaths in India… it's every parents' worst nightmare. Sadly for villagers in India this nightmare is their reality, a completely unacceptable reality.
So one evening, as I was clearing away my children's mountain of toys and emptying beakers of wasted milk, juice and water, it got me thinking… at what age should our children, the future generation with the power to force change, be aware of the plight of others? We, quite rightly go to huge lengths to protect their innocent minds from the horror stories that make the news headlines almost every day, but should we protect them from knowing about people in desperate need… people that we have the power to help in some small way?
We're all guilty of spoiling our children from time to time and I'm sure I'm not the only one who takes a simple glass of water for granted, but I believe it is my parental duty to ensure my children are grateful for what they have as well as having compassion for others in need. The trick is to find a way of nurturing this compassion without making them fearful of the world we live in.
That is why the Walking for Water '6 Mile Virtual Challenge' has come at exactly the right time for my 5 year old son, Harry.
So on Sunday 22nd October my son and a group of his friends will be taking on a 6 mile sponsored challenge for Jeevika Trust, to help give more children in India access to safe, clean water that we take for granted every day. Harry will be taking on the challenge by walking, scooting and cycling around a field behind our house – conveniently the farmers field is exactly 1 mile so he will be doing this circuit 6 times on the day.
He may only be 5 years old, and yes 6 miles is a long way BUT he has the heart and compassion of someone much older. He doesn't fully understand the extent of the poverty in Indian villages, and the horrors that go with it, and in all honesty I am keen to preserve his innocence for a little while longer. But he does understand that the money raised from this 6 mile challenge will go towards restoring reservoirs and building wells to stop women and children having to walk miles every day in extreme heat to fetch water in rural India. And in my opinion that is more than enough for someone his age!
I couldn't be prouder of Harry for taking on this challenge and I will be there every step of the way showering my amazing, kind hearted and compassionate boy with support, kisses and cuddles for doing something so wonderful for people less fortunate than himself.
So I urge you, if you're not able to join our Walking for Water event this Sunday then why not consider setting up a virtual 6 mile challenge with your children, pets and anybody else that might be interested. Not only will you be raising money for people who truly need it, but you'll always be teaching your children to have compassion, gratitude and most importantly teaching them that they have the power to make the world a better place.
Please do visit our Virtual 6 Mile Challenge page to find out more.
Why India is definitely NOT "too rich for aid"….


Epson pro EX9210 drivers is an application to control Epson Pro EX9210 1080p+ WUXGA 3,400 lumens color brightness wireless HDMI MHL 3LCD projector. The driver work on Windows 10, Windows 8.1, Windows 8, Windows 7, Windows Vista, Windows XP. Also on Mac OS X 10.14 (MacOS Mojave) MacOS High Sierra, MacOS Sierra, El Capitan, Yosemite, Mavericks, Mountain Lion, Lion and mobiles. You need to install a driver to use on computer or mobiles. For more information about this driver you can read more from Epson official website.
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0 Response to "Epson Pro EX9210 Driver Download Windows, Mac"


Can we use ontology for?
Natural language to Ontology (OWL, KIF etc.) or CNL converter?
How to begin an ontology of a parliament?
Guanilo's objection to the ontological argument.
How would you make research from quantitative perspective?
What is the meaning of thing?


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text:
Home All The News Pochettino: Son and Janssen will step up without Kane
Pochettino: Son and Janssen will step up without Kane
Date published: Friday 17th March 2017 2:30
Harry Kane feels optimistic about his ankle injury and has joked about returning in less than a month, according to Tottenham manager Mauricio Pochettino.
Spurs said on Tuesday the injury is considered less serious than the one Kane sustained in September, when he damaged the same ankle ligaments and was out for seven weeks.
Even if Kane is overly confident in hoping to return far sooner, his assessment suggests he could be back for next month's north London derby against Arsenal on April 30 and may even feature in the FA Cup semi-final against Chelsea on April 22.
The cup clash at Wembley will come six weeks after Kane sustained the injury against Millwall last weekend.
"He is very positive, joking about (coming back) after the international break, three to four weeks," Pochettino said.
"It's good but we need to be careful with the injury. We trust completely our doctor and physios and that department who look after them in the best way."
On Kane's prediction, Pochettino added: "We don't know. I express the feeling and the way we are doing on the training ground.
"He is very positive but don't take it like properly my words because if not four, it's five to six weeks. But the good thing he is very positive.
"If you are positive in your mind you can affect your injury positively."
Kane has been left out of Gareth Southgate's England squad for next week's matches against Lithuania and Germany while Tottenham will have to do without their star striker against Southampton on Sunday.
They may also have to cope without their two first-choice full-backs at White Hart Lane, given the club have revealed Kyle Walker twisted his ankle on a day off at home on Monday. Danny Rose is still recovering from a knee problem.
Pochettino would not divulge the cause of Walker's injury but said the defender had not trained this week and will have to be assessed. He is unlikely, however, to withdraw from the England squad.
Victor Wanyama is also struggling after enduring a "minor problem" against Millwall but Mousa Dembele, who missed the match with an ankle injury, is available. Erik Lamela remains sidelined with a hip injury.
Kane's absence, however, is the biggest concern for Pochettino, given Tottenham endured their worst period of the season while the 23-year-old was out in September and October.
Vincent Janssen and Son Heung-min will be charged with filling the void.
"We hope things will be different this time but it was a different period, the team is different now. We are finding our best. The team is more solid," Pochettino said.
"Today is a great chance for people like Son and Janssen to play more regularly in the starting XI. It's a great chance for them."
Son hit a hat-trick against Millwall last weekend while Janssen scored his first goal from open play since joining Spurs for £17.5million from AZ Alkmaar last summer.
Pochettino is backing both forwards to step up.
"When you have a striker like Harry Kane who scores and plays well it's difficult for offensive players to play," Pochettino said.
"Vincent is very young, came from Holland, a different league and the adaptation to the Premier League is always difficult. He is learning and improving, it's only his first season in England."
On Son, Pochettino added: "It is a big chance for him. The system we use in the last few months has not allowed him to play with maybe two or three strikers.
"But today Harry Kane is not available so he will have the chance to play more."
heung-min son mauricio pochettino spurs Tottenham Vincent Janssen
Man Utd look daft for many reasons. Selling Lukaku isn't one…
The Mailbox reckons Romelu Lukaku's sale was a win-win situation. Also: replies to 16 Conclusions, gambling, Chelsea, and more...
Gossip: Man Utd faff over Fernandes, another big six suitor for Grealish
Man Utd want a discount on Bruno Fernandes or to use two players in part-exchange. Meanwhile, Grealish is in demand...
Tottenham 0-1 Liverpool: Bobby dazzles as Reds ride luck
Firmino's superb touch and finish was the difference in north London.
January 11 2020, 12:50 pm
Here's comes Mourinho to halt Liverpool's march to Invincibility…
The Mailbox has a feeling about Jose some bad juju for Liverpool this weekend. Also: the Man Utd blame game...
Devastating blow for Spurs as they lose Kane until April
Tottenham have announced striker Harry Kane is set for surgery to repair a ruptured tendon in his left hamstring.
Gossip: Man Utd eye £50m midfielder and loan centre-backs
Man Utd reckon Ajax could be vulnerable to an offer for Donny van de Beek, while Spurs are in for a £30m-rated striker...


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Every summer during strawberry season, I take on the personal project of creating my own Jam packaging (and creating the jam too!) Each year I try and strike a completely different vibe. These are the labels I designed for the past two years.


text:
\section{Introduction}
Active Galactic Nuclei (AGN) are among the most powerful sources of radiation across the whole electromagnetic spectrum, from $\gamma$-rays (up to TeV energies in some cases) down to radio waves. Accretion onto a central supermassive black hole (SMBH) is generally accepted to be one of the dominant physical mechanisms that power these systems. Another source of energy is believed to be the rotational energy of the SMBH itself, which in some cases can exceed the gravitational energy extracted through accretion.

The radiation output of quasars and Seyfert galaxies peaks in the ultraviolet \citep{shakura73}, producing the so-called ``big blue bump'' in the spectral energy distribution (SED), while only a fraction of the energy available through accretion is reprocessed into high energy emission (from keV energies to hundreds of keV)  via thermal comptonization, which produces a second, less dominant peak in the SED, and which is generally thought to cause the cosmic X--ray background \citep[CXB,][]{giacconi62}. The most accepted scenario for  comptonization requires a population of hot electrons \citep[i.e. a corona, see][]{haardt91} that ``sandwiches'' the inner part (tens of gravitational radii $R_g = GM/c^2$) of the accretion disk, and which is kept hot by magnetic reconnection. Additionally, an outflow or a jet could contribute to the total emitted power, more prominently at radio frequencies through synchrotron radiation and less markedly at $\gamma$--ray frequencies \cite[see e.g.][]{teng11, lenain10}.

When AGN also produce relativistic jets which are pointing in the direction of the observer, they are referred to as blazars. In this subclass of AGN the SED shows two clear peaks, or ``humps''. In leptonic models, all the radiation we see coming from the central object is generally thought to be generated by a single population of electrons, i.e. directly or indirectly by the jet itself. This is achieved via synchrotron emission producing the lower--energy hump and via a combination of external compton (EC) and Synchrotron--self--Compton (SSC) producing the high energy hump. Only in a handful of cases the thermal radiation coming from the accretion disk is powerful enough to ``pierce'' through the synchrotron hump, and  could be used to estimate the mass and accretion rate of the AGN. All blazars are powerful radio sources, and the relative contribution of the two peaks in the SED as well as the position of their synchrotron peaks classify them into subclasses of radio (and total) power \citep{fossati98}.

In practice, a popular method of classifying AGN uses the ratio of the radio (at 5~GHz) to optical (at 4400~\AA) fluxes, through the so--called radio-loudness parameter $R=F_{radio}/F_{optical}$. Initially, the distinction between radio-loud ($R>10$) and radio-quiet ($R\lsim10$) objects  appeared sharp \citep{strittmatter80, kellermann89, kellermann94} if derived from the distribution of the $R$ parameter of AGN present in the Palomar Bright Quasar Survey. Up to five other similar proxies of R have been defined in the literature \citep[for a recent review see][and references therein]{elvis12}.
The existence of a bimodality has been ever since debated in the literature in favor \citep[see e.g.][]{miller90,stocke92,hooper95,ivezic02,jiang07} or against it \citep[see e.g.][]{condon80, white00, cirasuolo03, rafter09}. A possible source of confusion is the different size, sensitivity limits, cuts in redshift, optical and radio frequencies used to classify AGN through the R parameter.

Recently \cite{mahony12} used a soft X--ray selected sample of several hundreds quasars and did not find any evidence of bimodality. Seyfert galaxies are traditionally considered radio-quiet sources but, for example,  \cite{ho_peng01} showed that considering their nuclear luminosities, most Seyfert galaxies are radio-loud.

To account for this dichotomy, it was proposed that just rapidly spinning black holes can produce relativistic jets responsible for non--thermal emission \cite[e.g.][]{blandford90}. Nonetheless, in later years the evidence for high spin came from a radio--quiet object (MCG-6-30-15, \citealp{tanaka95}).
Other works \citep{nandra07, patrick12} showed that broad relativistic lines are frequently observed in Seyfert galaxies and in a handful of cases (e.g. NGC~3516, NGC~7469) they could also constrain the spin.
Other results are at odds with the idea of radio--quiet objects hosting slowly spinning black holes. One example is the high efficiency required by accretion in order to account for the integrated CXB \citep{elvis02}, which is more easily explained if the BH are spinning. Other examples are X--ray observations that indicate that the emission extends well within the innermost stable orbit of non--rotating black holes \citep[e.g.][]{fabian02, iwasawa96}.
Moreover, both Seyfert galaxies and low--luminosity AGN (LLAGN) were shown to be radio emitters at some level. For instance, \cite{ho_ulvestad01} have shown that 85\% of Seyfert AGN are detected at 5~GHz, with a wide range of radio powers and morphologies, where structures could be resolved by very long baseline interferometry (VLBI).
\cite{nagar02}, \cite{ulvestad03} and \cite{giroletti09} showed clear structures (blobs or knots) at the sub--parsec level.
The origin of radio emission at this level is not yet fully understood. In most cases it is
associated to synchrotron emission just as in the radio--loud case \citep{giroletti05,ishibashi10} and, if so, should highlight the presence of a jet or outflow also in this class of objects. Alternatively, thermal free--free emission is viable option \citep[see e.g.][for the radio emission of NGC~1068, among others]{gallimore04}.

The radio--X connection has been  addressed by different authors, but given the different energy ranges used in the high--energy band coupled with different radio frequencies, the results are often discordant (and will be discussed in Sect.~4). For instance, in the seminal work by \cite{merloni03} a relation between the  radio luminosity at 5~GHz and the X--ray 2--10 keV luminosity $L_R \propto L_X^{0.6}$ (i.e. $L_X \propto L_R^{1.7}$) was found and  a solid theoretical interpretation was discussed in relation to the scale invariance of black hole jets \citep[see also][]{heinz03}. Other authors find a slope close to unity \citep{canosa99, brinkmann00, salvato04, panessa07} or a completely different slope $L_X \propto L_R^{0.6}$ \citep{wang06}  similar to what observed in few Galactic black holes \citep{corbel13}.
While completing this paper, \citep{bonchi13} reported an updated version of the Fundamental Plane, with a slope even harder than the original one: $L_R \propto L_X^{0.39}$.

The aim of this work is to study \emph{for the first time} the radio--X connection in local Seyfert galaxies in the hard--X ray, high--frequency radio regime.  We want to test whether the correlation between the radio and X--ray power at high radio and X--ray frequencies is as strong as at lower frequencies, or conversely tends to vanish (as it seems to be the case when high resolution  Very Long Baseline Interferometry observations are used - Panessa \& Giroletti, 2013, MNRAS submitted). To these aims we cross--match the sources present in the BAT survey (15--55 keV) with the sources detected by the high frequency (20~GHz) Australia Telescope Compact Array (ATCA) survey.
A similar  complementary work is in progress \citep{panessa11} adopting the sample of AGN detected by the INTEGRAL satellite, and the 1.4~GHz radio luminosity.
Although our primary focus is on Seyferts, we also consider the blazars found through the cross--matching, in other to investigate the possible gap in the radio--to--gamma ray connection in blazars recently studied  \citep{mahony10, ghirlanda10b,ackermann11}.

Another approach to the present work is to investigate whether the correlations arise when long--term averages are used, or conversely if there is a radio--X connection at all scales. When at lower radio frequencies the ``core'' luminosities (albeit the ``core'' could mean jet structures of the order of kpc) are confronted to the high--energies the correlation holds both for pointed and survey (i.e. averaged) X--ray observations. Choosing higher radio--frequencies allow us to be less contaminated by the extended structures and therefore a shorter (but still somewhat averaged) radio output. We expect that if we compared hard X--rays from a survey telescope with lower radio frequencies \citep[see an example in][]{panessa11}, we would still recover a strong correlation, possibly because we would be confronting longer term averages, instrumental/observational in the case of X--rays and physical in the case of radio waves.
 Nevertheless, we note that there is a still large difference in the time scale for X--ray emission (years, for all--sky surveys) and radio waves (several thousand years in kpc--scale regions).
The best test we envisage for the future will be to investigate the radio--X connection using focussing hard X--ray telescopes like NuSTAR \citep{harrison10} and VLBI radio luminosities, which should both probe at the same time the very inner part of the AGN.

In Sect.~2 we briefly discuss the two surveys and the cross--correlation technique. We present our results in Sect.~3 and discuss them  in Sect.~4. We summarise our findings in Sect.~5. A standard flat Universe with $h=\Omega_{\Lambda}=$0.7 is assumed.

\section{The sample}
We give a brief description of the two blind surveys we used for this work, but we refer the reader to the respective original publications for a detailed discussion of both surveys' strategies and peculiarities. In \S~\ref{sect:associations} we describe the cross--correlation technique we adopted.

\subsection{The \textit{Swift}/BAT survey}
The Burst Alert Telescope \citep[BAT;][]{barthelmy05} instrument on--board the \textit{Swift}\ satellite \citep{gehrels04} is a coded mask instrument originally thought to alert the X--ray and Optical--UV cameras to follow-up $\gamma$--ray burst afterglows. While surveying the sky waiting for a trigger, the BAT continuously monitors up to 80\% of the sky thanks to its wide field of view ($120^{\circ} \times 90^{\circ}$ partially coded). After several years of deep exposure, the BAT survey covers almost uniformly the whole sky down to the limiting sensitivity. In our analysis we used the data accrued in 6 years  of exposure, down to a sensitivity limit $\sim 6\times10^{-12}$ erg/cm$^2$/s. The BAT survey is presently \citep[see][for the latest release]{ajello12} the deepest blind scan in the sky above 10~keV making it the optimal candidate for the goal of confronting the hard X--ray and radio properties of AGN.
\begin{figure}
\hspace{-0.5cm}
\includegraphics[width=9cm]{prob_ass.eps}
{\caption{Association (posterior) probability between the \textit{Swift}/BAT and AT20G samples versus radio flux density and hard X--ray flux of the matched sources. Two `outliers' are clearly visible in the low-flux low-probability section of the data cube. These are the only two AGN for which the association probability is between 80\% and 95\%. }
\label{probass} \vfil}
\end{figure}
Data screening and processing were described in details in \cite[][A08a]{ajello08a} and \cite[][A08b]{ajello08b} but we summarise hereafter the main characteristics of the survey. The chosen energy interval for (conservatively) computing the fluxes was 15--55 keV, while the spectra are traditionally extracted in the 15--200 keV energy range. The all--sky image was obtained by averaging the (weighted) per--pointings, resulting in a final sample of $\approx 350$ AGN, comprising mostly Seyfert--like galaxies (284) and blazars.
Just $\sim5\%$ of the sources of the BAT catalogue still escape  identification, and this incompleteness is independent of the Galactic latitude \citep[see e.g.][]{ajello12}.
Each of these sources has a signal--to--noise ratio $SNR \gsim 5\sigma$, and was identified by cross--matching it against the previous catalogues of \cite{tueller08}, \cite{cusumano10}, \cite{voss10}, and \cite{burlon11}. Whenever possible, optical identifications were taken from \cite{masetti08, masetti09, masetti10} as described in \cite{ajello12}. For the blazars we checked their classification against the BZCAT\footnote{http://www.asdc.asi.it/bzcat/} catalogue \citep{massaro09}.

\subsection{The AT20G survey}
The AT20G survey \citep{murphy10} is one of the largest blind surveys at high radio frequencies ever conducted from ground. It covers $\sim 20,000$ deg$^2$ to a limiting flux density of 40 mJy/beam. The key feature of the survey was its two--phase strategy, where a fast blind scan (possible due to the fast--scanning mode of the Australian Telescope Compact Array) was followed by regular snapshots by the ATCA.

\begin{figure}
\includegraphics[width=\columnwidth]{alfalfa.eps}
{\caption{Scatter plot of the radio spectral indices of the all AT20G sources are shown in red crosses. Seyfert galaxies (blazars) are shown with circles (squares). The two panels show the (arbitrarily rescaled) projected distributions along the respective axis of the whole AT20G population (red histogram) and the whole cross-correlated subsample (black histogram).}
\label{alfalfa} \vfil}
\end{figure}

In the first phase the ATCA scanned the whole \emph{southern} sky at 20~GHz, with a speed of $15^{\circ}$~min$^{-1}$ in declination at the meridian. The scanning strategy exploited the Earth rotation, while sweeping regions of the sky $10^{\circ}-15^{\circ}$ wide in declination. The rms sensitivity of the first phase was $\simeq 10$~mJy. In the second phase, the sources brighter than $5\sigma$ where followed--up with an hybrid array configuration and two 128 MHz bands, combined during data processing at the central frequency of 19.904~GHz (that we refer to as 20~GHz throughout the paper). The sources with declination~$< -15^{\circ}$ were observed also at 4.8~GHz and 8.64~GHz (which we refer to as 5~GHz and 8~GHz), with an east--west configuration. The exclusion of sources with declination $> -15^{\circ}$ for the lower frequencies is motivated by the poor $(u,v)$ coverage of east--west arrays near the equator.

\begin{figure*}
\includegraphics[width=\columnwidth]{ksflux_BAT.eps}
\includegraphics[width=\columnwidth]{ksflux_20GHz.eps}
{\caption{Distribution of the parent populations flux, compared with the associated AGN. The distributions have been rescaled.
\textit{(Left:)} \textit{Swift}/BAT flux in the energy band 15--55 keV for the whole 6--year catalog (thin line) and the associated subsample (thick dashed line).
\textit{(Right:)} AT20G flux densities at 20~GHz, with the same notation as left panel.}
\label{ksflux} \vfil}
\end{figure*}

\subsection{Source Associations} \label{sect:associations}
For the positional cross--matching of the BAT and AT20G source catalogs we adopt a Bayesian method already used in cross--matching the \textit{Fermi} AGN with the AT20G survey \citep{ghirlanda10b} and first developed for the identification of the {\it Fermi} sources \citep[][and references therein]{abdo10a}.
This method, given the BAT source position and accuracy (which we assume to be half of the point spread function) assigns a probability to every radio source found within the BAT error circle. This probability is computed accounting for the surface density of radio candidates around each BAT source. To this aim, the prior probability of the radio sources (i.e. the confidence that the radio catalogue contains the counterpart of the X--ray selected AGN) is calculated as per appendices B and C of \cite{abdo10a}, and is assumed equal for all the sources. In practice, this translates into calculating the average number of false associations between the AT20G catalogue and 100 randomly generated mock X--ray catalogues.
{Similarly to what done in  \cite{abdo10a} and \cite{ghirlanda10b}, we call an `association' a unique match (i.e. a single radio source within the BAT error circle) with a posterior probability greater than 80\%.
We comment below on some of the sources that are flagged in the original paper by \cite{murphy10}. While this method allows us to derive a figure of merit for the associations found in the two catalogs, we note that by only searching for positional matches (i.e. radio sources within the BAT error circle), we could derive a similar --albeit smaller-- number of associations.

\input{tabellon.tex}

We find 37 BAT AGN with a radio counterpart in the AT20G survey. Not surprisingly the blazar class has a detection rate of $\approx 65\%$, which is much higher than the equivalent for Seyfert galaxies, i.e. $\approx 14\%$. These are listed in Table~\ref{tabellon}, along with the posterior probability of the association. About half of the associations (19/37) are classified as Seyfert galaxies, roughly equally distributed into the two subclasses of optically Seyfert ``type 1'' (7, plus 1 Sy1 Narrow Line) or ``type 2'' (11). There are 18 AGN classified as either BL Lacs (1) or FSRQ (15) blazars, and 2 classified as generic blazar type. The absolute majority of the FSRQ class is no surprise, given that our parent sample is the \textit{Swift}/BAT one, which is well known to pick preferentially this class of AGN.
Note that all but two Seyfert 2 AGN (i.e. ESO 549-G049 and ESO 157-G023) have a probability in excess of 95\%, and that both the less certain associations are close to the detection limit of both surveys. This is represented in Fig.~\ref{probass}, where the two sources are clearly displaced from the bulk of the associations.

\emph{Properties of the cross--matched sample:}
One of the results of the AT20G survey is that a large fraction of sources are not well fit by a single power law even in the small bandpass of the ATCA telescope. In Fig.~\ref{alfalfa} we show the distribution of the spectral index of the several thousands sources of the AT20G for which the spectral index could be  computed \citep[see for comparison][]{murphy10, massardi11}. In the same plot we show the radio spectral indices of the BAT sources associated to the radio counterparts.
The spectral indices where calculated in the standard way taking from \cite{murphy10} the flux densities ($S$) at frequencies $\nu_1$ and $\nu_2$:
$$ \alpha_{12} = \frac{log_{10}(S(\nu_1)/S(\nu_2))}{log_{10}(\nu_1/\nu_2) } $$
Fig.~\ref{alfalfa} shows that the associations we found do no show a particular spectrum, i.e. they populate all the four quadrants of the plane identified by the dashed lines corresponding to $\alpha = -0.5$ which is often adopted as a separation between hard and soft radio sources. \cite{chhetri12} pointed out that AT20G is a high frequency survey and hence it has a larger fraction of flat--spectrum compact radio sources ($\sim 80$\%) than the surveys at lower frequencies ($\sim 25$\%).

We checked also whether the association method tended to pick the brighter end of the distribution of both populations. In Fig.~\ref{ksflux} we show that albeit this is not true for the hard X--ray population, it seems that the radio part of our association picks up preferentially  brighter sources.
When we compare the \textit{Swift}/BAT flux distributions (left panel), it is apparent how this work is sampling AGN which are on average distributed exactly as the parent population. When we look at the 20~GHz flux distributions, the associated AGN have a flat distribution. Note that we chose to compare the flux densities at 20~GHz because this is the most sampled frequency of the radio survey (the follow--up completeness is $>90\%$ only above 100 mJy, see \citealp{massardi11}).
\begin{figure}
\includegraphics[width=\columnwidth]{radio20x_flux.eps}
{\caption{Scatter plot of the \textit{Swift}/BAT flux in the energy band 15--55 keV vs. 20~GHz flux density. The sensibilities of the two surveys are represented with the grey shaded area. Seyfert galaxies are plotted with blue open (red filled) circles if their flux from the six-year BAT survey (unabsorbed as per \citealp{burlon11}) is used. Blazars are represented with black squares (FSRQ), crosses (BL Lac), and diamonds (unclassified).}\label{20ghz_flux} \vfil}
\end{figure}

\emph{Notes on `extended' sources\footnote{In the original AT20G catalog 5 of our sources were originally flagged as `poor'. Their flux density measurements are anyway unaffected due to the method (referred to as \textit{Triple Product Method}; see \citealp{murphy10} for additional details) used, which is robust against the effects of decorrelation (phase fluctuations of the visibilities). These flagged data have no significant effect for the analysis.}:}
\cite{massardi08} reported that the radio galaxy Fornax~A (that is not present in our sample) is the only bright extragalactic source known to be missing from the AT20G. This incompleteness is a result of its 20~GHz flux coming from the lobes being resolved by the ATCA beam. In our sample 6 sources (2MASX~J04450628--2820284, NGC~1068, Circinus, PKS 2356--61, IGR J03532--6829, ESO--362-G021) are flagged as 'extended', while 3 additional ones (Cen~A, Pictor~A, NGC~612) are additionally flagged as `large and extended'.
Note that the AT20G is known to be biased against extended sources due to a reduced sensitivity (50\% reduction in amplitude for source size $>45$~arcsec) and all these sources were targeted specifically by \cite{burke09}, see in particular their Table~2. Their total integrated flux measurements are reported in the catalogue we are using in this work, so that when we compare with the compact sources, we are not underestimating the flux densities of the former. In practical terms, we are using the flux coming from the innermost 1--2~kpc of the source (e.g. for Cen~A the scale is 0.037 kpc/arcsec, which means that the 20~GHz flux densities refer to the innermost 1.57~kpc, i.e. the core of the active galaxy and the initial part of the jets that extend for $\gsim$~1~Mpc). Also \cite{murphy10} comment further on this, in the context of associating the radio emission with the core of NGC~1068 (and other close galaxies), and point out that the reported flux appears to be associated with the active nucleus.

\section{Results}
We explored the possible correlation between the hard X--ray flux (15--55 keV) and the radio flux density at 20GHz. Fig.~\ref{20ghz_flux} shows the scatter plot for the associations. There is no correlation between the two quantities for the Seyfert galaxies as also confirmed by the Spearman's rho correlation coefficient $r_s = 0.38$ (corresponding to a chance correlation probability $P= 0.11$). This correlation is even weaker if we include the blazars. Therefore we find no evidence of a relation between the fluxes.

Note that four associations are Compton--thick sources: NGC~612 and NGC~1068 (both present in \citealp{burlon11}), NGC~4945, and Circinus. We show their absorbed and unabsorbed\footnote{For NGC~4945 and Circinus we estimated the suppression factor using the prescriptions of \cite{burlon11}, which are consistent with the findings of \cite{brightman11}. To this aim we used a fiducial value of $N_H$  taken from the most recent literature (\citealp{yaqoob12} and \citealp{dellaceca08}, respectively)}
X--ray fluxes (connected by a vertical dashed line) in Fig.\ref{20ghz_flux}.}

We over--plotted in Fig.~\ref{20ghz_flux} the two limiting fluxes of both surveys as a grey shaded areas. The absence of points in the upper part of the plane does not seem affected by a simple selection effect, while the lower right one is likely affected by the BAT sensitivity.

\begin{figure*}
\includegraphics[scale=0.75]{radio20x_lum.eps}
{\caption{\textit{Swift}/BAT luminosity vs. AT20G radio luminosity at 20~GHz. Different sources as per the legend and Fig.~\ref{20ghz_flux}. The best (bisector) fits are shown with a dashed blue, dash-dot, dash-triple-dot line for the Seyferts, all sample, and blazar respectively. The dotted lines represent three different $R_X$ values of 0.01, 0.1, 1 and are conversely expressed in the bottom left of the corner as relative radio--X luminosities. }\label{20ghz_lum} \vfil}
\end{figure*}

However, the study of the correlation between the power output at different frequencies is often done in the luminosity space rather than in the flux space.
We computed the $k$--corrected BAT luminosities via:
$$L_{\mathrm{BAT}} = 4\pi d_{\rm L}(z)^2 \frac{F_{15-55}}{(1+z)^{2-\Gamma}} $$
where $\Gamma$ is the photon index of the individual source fitted in the whole BAT energy band. Note that the usual notation of the X--ray photon indices is such that $F(\nu) \propto \nu^{1-\Gamma}$.
The $k$--corrected radio luminosity at the $i$--th central frequency (19.904~GHz, 8.64~GHz and 4.8~GHz) was obtained from the flux density $S(\nu)$ via:
$$L_{\mathrm{AT20}} = 4\pi d_{\rm L}(z)^2 \frac{\nu_i \times S(\nu_i)}{(1+z)^{1+\alpha}} $$
where $\alpha$ is the energy spectral index
$(S(\nu) \propto \nu^{\alpha})$,
so that we are calculating both luminosities in units of erg/s. We chose to use the spectral index between 5~GHz and 20~GHz as a proxy of the radio spectrum in the available ATCA band. We used the median spectral index for the sources which lacked the flux density measurement at 5~GHz.
A caveat for the more distant sources is that \cite{chhetri12} showed that the AT20G sources tend to show a turn over at the rest--frame frequency of about 30~GHz. This curvature effect does not significantly impact the $k$--corrected luminosities for all but the sources\footnote{For SWIFT~J1656.3--3302, SWIFT~J0539.9--2839, PKS~2126--158, QSO~B2052--47, PKS~0524--460 the radio luminosity is strictly speaking a lower limit.}
which are at high redshift ($z \gsim 1$) and harder than $\alpha=-1$.

The result is shown in Fig.~\ref{20ghz_lum}. The $L_{\mathrm{BAT}}$--$L_{\mathrm{AT20}}$\ correlation appears  stronger with respect to the flux plane, as can be seen in the corresponding Spearman's rho correlation coefficients and chance correlation probabilities (see the top panel of Table~\ref{tab:statistics}).
A fit with the bisector method at 20~GHz yields
$$logL_{X}= 0.68(\pm 0.11)\,logL_R + 15(\pm 5)$$
for the Seyfert sample, which is consistent with the slightly flatter result we obtain including also the blazars
$logL_{X}=0.75(\pm 0.05)\,logL_R + 12(\pm 2)$.

\input{pca.tex}

However, the common dependence of the radio and X--ray luminosities with redshift should caution about the significance of the correlations. In order to remove the effect of $z$ we performed a partial correlation analysis, as detailed in the appendix.
 We find that the correlation is not significant for the sample of Seyfert--like AGN (chance correlation probability is 78\%). The apparent relation is therefore completely driven by their distance modulus. A caveat when considering the whole sample: from a purely statistical point of view the null hypothesis probability is $\sim 2 \times 10^{-2}$, corresponding to a confidence of 2.4\,$\sigma$. Nonetheless, since the redshift distribution is almost bimodal, we are effectively computing the partial correlation among two different populations. The Seyfert one with a lower median flux and distance versus the blazar one, with a much higher median flux and redshift. The results of the analysis in all the three available radio bands is summarised in Table~\ref{tab:statistics}.

\section{Discussion}

There is a natural scenario in which all X--ray emitting AGN are also radio emitters at some level, i.e. a scenario in which all AGN are able to accelerate a jet, even though only a small fraction ($\sim 10\%$, the genuine radio--loud) are able to successfully launch such a jet. In this ``aborted--jet'' scenario \citep{ghisellini04}, most AGN are indeed unable to launch the jet due to its subrelativisic speed, which make the jet collapse back and account for both radio and high--energy emission. The difference with the more well--known accretion scenario is due to the heating mechanism for the electrons responsible for the X--rays, which in the case of an aborted jet, is predicted to be localised along the (failed) jet axis. It is worth nothing that both scenarios are not necessarily in competition with each other, and may well be both contributing at different levels in the radio and high--energy bands.

It is not surprising that lot of effort has been spent investigating the reciprocal contribution of radio emission and X--rays. In recent years numerous groups have tackled this issue from different perspectives.
Different authors used soft X--ray \citep{canosa99, brinkmann00, salvato04}, and found a slope of the correlation which is close to unity\footnote{The slope is consistent with unity for \cite{brinkmann00} if the radio--quiet sample is considered.}. Some differences among the different works emerge as a consequence of the fitting method, and/or of the inclusion of some AGN which might be contaminated by a starburst component, and/or the definition of radio--loudness (as discussed before). \cite{canosa99} adopted monochromatic X--ray luminosities at 1~keV for a sample of $\sim 40$ ($z<0.1$) AGN. \cite{brinkmann00} chose 2~keV luminosities for $\sim 60$ ($z<1$) AGN , respectively. These were compared to the 5~GHz luminosity and a significant correlation was found (even if the effect of distance might have been underestimated). In the work of \cite{salvato04}, 53 local ($z < 0.1$) AGN were cross--correlated in the X--ray energy band of 0.5--2~keV versus 1.5~GHz monochromatic luminosities.

Another difference emerges when we consider that the lower the radio frequency we adopt, the more we are contaminated by the lobes which reside further out. To the aim of checking the existence and validity of a relation between the jet output at radio and X--ray frequencies, shorter wavelengths are to be preferred.
\cite{panessa07} studied an optically selected sample of $\sim$50 Seyfert galaxies, and compared the 2--10 keV luminosities to the 1.4, 5, and 15~GHz ones. In particular they found that the best fitting relation, taking into account also censored data, is represented by the same relation that holds for a sample of LLAGN, with a slope of between 0.71 and 0.97 at 5~GHz, and 0.8 and 1.02 at 15~GHz, with (without) the inclusion of a few radio--loud sources (according to the definition of \citealp{terashima03}) respectively. The difference between their Seyfert sample and the LLAGN is the mass range, which \cite{merloni03} showed to be the third parameter in the so--called ``fundamental plane of black holes'', which is anyhow only a scale parameter. It is worth noting that \cite{degasperin11} found only a mild relation in faint LLAGN between 2--10 keV X--rays and 4.8~GHz and 8.4~GHz.
\begin{figure}
\includegraphics[width=\columnwidth]{rx_20.eps}
\caption{Distributions of the $R_X$ parameter.} \label{rx}
\end{figure}

The framework of the ``fundamental plane of black holes'' is to establish both theoretically and observationally the coupling between the disk (i.e. the accretion power) and the jet. To that aim the accretion power linked to the X--ray emission from the corona and the radio power is associated to the jet. One of the result of their work is to successfully interpret their findings in the framework of the fundamental connection between a radiatively \emph{inefficient} accretion flow and the jet, under the assumption of scale invariance of the jet \citep{heinz03}. From an observational point of view they proved that this coupling holds at all scales (i.e. both for AGN and Galactic black holes).

The absence of the radio--X correlation in our hard X--ray selected sample is at odds with the equivalent works at lower radio frequencies and lower X--ray energies. In principle this could be due to either an incompleteness of our sample (our result arises when cross--correlating $\sim 20$ AGN), or be physical in nature.
We checked if the relation was weaker or stronger at different radio frequencies. Not all sources have counterparts in the AT20G at lower frequencies, but as we show in Table~\ref{tab:statistics} the result seems to hold at 8~GHz and 5~GHz. We looked at even lower frequencies,  using the fluxes from the NRAO VLA Sky Survey \citep[NVSS;][]{condon98},  Sydney University Molonglo Sky Survey \citep[SUMSS;][]{mauch03}, and MGPS-2 \citep{murphy07}, but unfortunately just 8 Seyfert AGN can be securely associated to our selection. These numbers are too low to run any meaningful statistical analysis. The problem of having too few counterparts to our cross--matched sample at lower frequencies, is mirrored at higher frequencies. We also checked the 30~GHz and 40~GHz flux densities from the Planck satellite Early Release Compact Source Catalog \citep{planck11} v--1.3\footnote{http://irsa.ipac.caltech.edu/Missions/planck.html}. Less than 5 Seyferts among our sources have high frequency measurements, making the higher frequency analysis even less significant.

Motivated by the similar result of absence of correlation when using the VLBI radio luminosities (Panessa \& Giroletti, 2013, MNRAS submitted), we run the following check on our sample. By using the definition of compactness adopted by \cite{chhetri12}, we excluded from our analysis the sources whose visibilities of the longest--over--shortest baselines were smaller than 0.86. This effectively translates in a factor of $\sim 10$ better angular resolution, down to 0.15 arcsec resolution\footnote{This translates into structures more compact than $\sim 9$ pc at the median Seyfert redshift, and $\sim 1.3$ kpc at the median blazar redshift}.
Out of the whole sample, 21 AGN survive this selection and again the correlation is absent at the same statistical level to the original analysis.
Therefore we conclude that, if the absence of the correlation at high frequencies and high angular resolution will be proven statistically solid by future works, it could mean that the known radio--X correlation is relating a genuine ``core'' property (the X--rays) with a more distant one arising from the lobes of the jet. This in turn would imply that the X--ray output of  the AGN, averaged over the duration of the used survey, correlate with the energy reservoir represented by the distant radio structures.

\emph{Beamed sources:} Note that \cite{merloni03} excluded the radio--loud (blazar--like) objects, and so do most authors. This is because in the blazar case both luminosities are associated to the relativistic jet and therefore the electromagnetic output is boosted by a factor $\propto \Gamma^2$. This is not normally the case for Seyfert galaxies, in which the jet --if present-- is assumed to be sub--relativistic. Testing the universality of the disk--jet coupling at yet other scales is beyond the scope of this paper.
At the same time, they were motivated by the fact that the radio--X connection described by low mass systems and high mass systems defined parallel tracks in the luminosity plane. Indeed more massive objects like active galaxies tend to be more radio--loud with respect to the X--ray output when compared to Galactic black holes. The mass segregation and the accretion rate are in fact two important parameters of their treatment. It is nonetheless interesting to note a similar effect in our sample, if we compare the occupation of BAT selected Seyfert--like AGN and BAT selected FSRQ. In Fig.~\ref{20ghz_lum} we draw with dotted lines different radio--to--X ratios. Seyfert--like AGN tend to populate the area where the radio power is between 0.01 and 0.1 the X--ray power, while blazars tend to populate the more ``radio loud'' area where the ratio is between 0.1 and 1.

Another way to visualise this effect is to take the definition of radio loudness adopted by \cite{terashima03} adopting a similar ``high frequency'' radio loudness $R_X \equiv log(L_R/L_X)$. Fig.~\ref{rx} shows that the distribution of the $R_X$ parameter is different for the two classes of sources, which is a reflection of the two samples being displaced along different tracks. The median (and dispersion) of $log(R_X)$ for local Seyferts and blazars are  -1.88 (0.69), and -0.68 (0.34), respectively. The null hypothesis of the two populations of being drawn by the same parent sample has a probability $P=1.5 \times 10^{-4}$.

Our decision to include also the blazars in this work was to discuss the following: if the distribution of the Lorentz factors of the jets is peaked (i.e. if there is a ``typical'' $\Gamma$ for BAT FSRQ), then the beaming should impact the normalisation of the correlation drawn by their luminosities rather then the slope. Conversely, one has to consider that probably the dissipation of the jet power takes place in different areas along the jet, therefore the beaming will be different (higher) for the X--ray luminosities than for the radio luminosities. This effect likely affects also the slope of the correlation, but cannot be taken into account unless one independently knows the beaming factors for radio and X--rays.
Even if beyond the goal of this paper, we would like to mention that if such a control on the Lorentz factors could be obtained (e.g. from variability in X--rays with the NuSTAR satellite \citep{harrison10}, and from VLBI in radio), then we would be able to de--boost the luminosities of blazars, and compare them properly with the Seyfert ones.

\section{Summary and conclusion}
Starting from the six--year \textit{Swift}/BAT survey of AGN, we looked for counterparts at high frequency radio in the AT20G survey \citep{murphy10} of the southern sky. By adopting a Bayesan cross--matching algorithm we found 37 AGN active in both regimes. Both surveys are biased towards bright objects, given that the sensitivity of the BAT is of the order of $6\times10^{-12}$ erg/cm$^2$/s and the AT20G has a cut at 40~mJy.
At the same time, the use of high energy X--rays is basically unbiased with respect to intervening gas, while the use of the highest radio frequency available helps in the contamination of the radio fluxes by extended structures. This is the best available set of observations (excluding VLBI) at these frequencies, in order to confront the ``core'' properties of AGN.
We summarise our findings in the following:
\begin{itemize}
\item 	We investigated the radio--X connection at --so far-- unexplored X--ray frequencies \citep[but see][]{panessa11};
\item 	We found that only $\sim$20\% (considering that the AT20G covers the southern sky) of the hard X--ray AGN have a counterpart at 20~GHz, and these are equally distributed between local Seyfert galaxies and distant blazars;
\item 	The existence of a relation between the X--ray and radio output of Seyfert--like AGN in the form $L_X \propto L_R^{0.68}$ is essentially determined by the redshift;
\item	The revised radio loudness parameter shows a bimodality between the two classes of sources. A transition between the two could be ascribed to the fact that we are using a flux--limited sample, beamed luminosities for one class, and to a different mass distribution of these sources.
\end{itemize}

With the advent of the first focussed hard X--ray mission \cite[NuSTAR;][]{harrison10} there could be the interesting possibility to target the pre--selected sample of \textit{Swift}/BAT AGN and get a lower limit on the Lorentz factor of the high--energy emission. From extensive VLBI measurements we would be able to resolve the very base also of Seyfert radio jets \cite[see e.g.][]{giroletti09} and even constrain the beaming factor of the radio luminosity.
This will in principle allow the testing of the radio--X connection for both Seyfert and blazars at the same time, down to an hard X--ray sensitivity 100 times deeper than the current limit.

\section*{Acknowledgments}
DB is funded through ARC grant DP110102034.
DB thanks R. Ekers and F. Panessa for fruitful discussions and useful feedback.
This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration, and the SIMBAD database, operated at CDS, Strasbourg, France. Finally it has benefitted from extensive use of TOPCAT\footnote{http://www.star.bristol.ac.uk/$\sim$mbt/topcat/}.

redpajama_set_name: RedPajamaArXiv


I love the beginning of July…watching the kids coast into a slower pace with each day stretching out before them, a new adventure to be had.
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