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Printed from https://ideas.repec.org/a/wly/hlthec/v27y2018i2pe120-e138.html
The impact of spousal bereavement on hospitalisations: Evidence from the Scottish Longitudinal Study
Fu‐Min Tseng
Dennis Petrie
Shaolin Wang
Colin Macduff
Audrey I. Stephen
Dennis James Petrie
This paper estimates the impact of spousal bereavement on hospital inpatient use for the surviving bereaved by following the experience of 94,272 married Scottish individuals from 1991 until 2009 using a difference‐in‐difference model. We also consider the sample selection issues related to differences in survival between the bereaved and non‐bereaved using a simple Cox Proportional‐Hazard model. Before conducting these estimations, propensity score approaches are used to re‐weight the non‐bereaved to generate a more random‐like comparison sample for the bereaved. We find that those bereaved who survive are both more likely to be admitted and to stay longer in hospital than a comparable non‐bereaved cohort. Bereavement is estimated to induce on average an extra 0.24 (95% CI [0.15, 0.33]) hospital inpatient days per year. Similar to previous studies, we estimate the bereaved have a 19.2% (95% CI [12.5%, 26.3%]) higher mortality rate than the comparable non‐bereaved cohort.
Fu‐Min Tseng & Dennis Petrie & Shaolin Wang & Colin Macduff & Audrey I. Stephen, 2018. "The impact of spousal bereavement on hospitalisations: Evidence from the Scottish Longitudinal Study," Health Economics, John Wiley & Sons, Ltd., vol. 27(2), pages 120-138, February.
Handle: RePEc:wly:hlthec:v:27:y:2018:i:2:p:e120-e138
DOI: 10.1002/hec.3573
File URL: https://doi.org/10.1002/hec.3573
Petrie, Dennis & Allanson, Paul & Gerdtham, Ulf-G., 2011. "Accounting for the dead in the longitudinal analysis of income-related health inequalities," Journal of Health Economics, Elsevier, vol. 30(5), pages 1113-1123.
Dennis Petrie & Paul Allanson & Ulf-G Gerdtham, 2010. "Accounting for the dead in the longitudinal analysis of income-related health inequalities," Dundee Discussion Papers in Economics 248, Economic Studies, University of Dundee.
Petrie, Dennis & Allanson, Paul & Gerdtham, Ulf-G, 2011. "Accounting for the dead in the longitudinal analysis of income-related health inequalities," Working Papers 2011:9, Lund University, Department of Economics.
Petrie, Dennis & Allanson, Paul & Gerdtham, Ulf-G, 2010. "Accounting for the dead in the longitudinal analysis of income-related health inequalities," SIRE Discussion Papers 2010-98, Scottish Institute for Research in Economics (SIRE).
Herbert J A Rolden & David van Bodegom & Rudi G J Westendorp, 2014. "Changes in Health Care Expenditure after the Loss of a Spouse: Data on 6,487 Older Widows and Widowers in the Netherlands," PLOS ONE, Public Library of Science, vol. 9(12), pages 1-17, December.
Andrew J. Oswald & Nattavudh Powdthavee, 2008. "Death, Happiness, and the Calculation of Compensatory Damages," The Journal of Legal Studies, University of Chicago Press, vol. 37(S2), pages 217-251, June.
Oswald, Andrew J. & Powdthavee, Nattavudh, 2007. "Death, Happiness, and the Calculation of Compensatory Damages," IZA Discussion Papers 3159, Institute of Labor Economics (IZA).
Oswald, Andrew J. & Powdthavee, Nattavudh, 2007. "Death, Happiness, and the Calculation of Compensatory Damages," Economic Research Papers 269776, University of Warwick - Department of Economics.
Oswald, Andrew J. & Powdthavee, Nattavudh, 2007. "Death, Happiness, and the Calculation of Compensatory Damages," The Warwick Economics Research Paper Series (TWERPS) 827, University of Warwick, Department of Economics.
van den Berg, Gerard J. & Lindeboom, Maarten & Portrait, France, 2011. "Conjugal bereavement effects on health and mortality at advanced ages," Journal of Health Economics, Elsevier, vol. 30(4), pages 774-794, July.
van den Berg, Gerard J. & Lindeboom, Maarten & Portrait, France, 2006. "Conjugal Bereavement Effects on Health and Mortality at Advanced Ages," IZA Discussion Papers 2358, Institute of Labor Economics (IZA).
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Christakis, Nicholas A. & Iwashyna, Theodore J., 2003. "The health impact of health care on families: a matched cohort study of hospice use by decedents and mortality outcomes in surviving, widowed spouses," Social Science & Medicine, Elsevier, vol. 57(3), pages 465-475, August.
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Michaud, P.C. & van Soest, A.H.O., 2008. "Health and wealth of elderly couples : Causality tests using dynamic panel data models," Other publications TiSEM fdba31e1-0443-4f73-b4cc-b, Tilburg University, School of Economics and Management.
Michaud, P.C. & van Soest, A.H.O., 2004. "Health and Wealth of Elderly Couples : Causality Tests Using Dynamic Panel Data Models," Discussion Paper 2004-81, Tilburg University, Center for Economic Research.
Michaud, P.C. & van Soest, A.H.O., 2004. "Health and Wealth of Elderly Couples : Causality Tests Using Dynamic Panel Data Models," Other publications TiSEM 78233391-0993-415b-8a8e-a, Tilburg University, School of Economics and Management.
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Jalan, Jyotsna & Ravallion, Martin, 2003. "Estimating the Benefit Incidence of an Antipoverty Program by Propensity-Score Matching," Journal of Business & Economic Statistics, American Statistical Association, vol. 21(1), pages 19-30, January.
Jyotsna Jalan & Martin Ravallion, 2000. "Estimating the Benefit Incidence of an Antipoverty Program by Propensity Score Matching," Econometric Society World Congress 2000 Contributed Papers 0873, Econometric Society.
Fu-Min Tseng & Dennis Petrie & Roberto Leon-Gonzalez, 2014. "The impact of spousal bereavement on self-assessed health status: evidence from the Taiwanese elderly population," GRIPS Discussion Papers 14-13, National Graduate Institute for Policy Studies.
Simeonova, Emilia, 2013. "Marriage, bereavement and mortality: The role of health care utilization," Journal of Health Economics, Elsevier, vol. 32(1), pages 33-50.
Duan, Naihua, et al, 1983. "A Comparison of Alternative Models for the Demand for Medical Care," Journal of Business & Economic Statistics, American Statistical Association, vol. 1(2), pages 115-126, April.
Waldron, Ingrid & Hughes, Mary Elizabeth & Brooks, Tracy L., 1996. "Marriage protection and marriage selection--Prospective evidence for reciprocal effects of marital status and health," Social Science & Medicine, Elsevier, vol. 43(1), pages 113-123, July.
Stroebe, Margaret Susan & Folkman, Susan & Hansson, Robert O. & Schut, Henk, 2006. "The prediction of bereavement outcome: Development of an integrative risk factor framework," Social Science & Medicine, Elsevier, vol. 63(9), pages 2440-2451, November.
Everding, Jakob & Marcus, Jan, 2020. "The effect of unemployment on the smoking behavior of couples," EconStor Open Access Articles, ZBW - Leibniz Information Centre for Economics, pages 154-170.
Jakob Everding & Jan Marcus, 2020. "The effect of unemployment on the smoking behavior of couples," Health Economics, John Wiley & Sons, Ltd., vol. 29(2), pages 154-170, February.
Jakob Everding & Jan Marcus, 2019. "The Effect of Unemployment on the Smoking Behavior of Couples," SOEPpapers on Multidisciplinary Panel Data Research 1037, DIW Berlin, The German Socio-Economic Panel (SOEP).
Everding, Jakob & Marcus, Jan, 2019. "The effect of unemployment on the smoking behavior of couples," hche Research Papers 2019/17, University of Hamburg, Hamburg Center for Health Economics (hche).
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Canada's Justin Trudeau refuses to resign over claims of interference in bribery trial
Canada's ex-justice minister has said the prime minister's inner circle tried to pressure her into helping a Montreal-based firm in a graft case. The opposition urged a police probe with Trudeau dodging calls to resign.
Canadian opposition asked the federal police to investigate possible political meddling by Justin Trudeau's government in a corruption case on Thursday. Previously, Trudeau's former justice minister Jody Wilson-Raybould accused Trudeau and his senior aids of "hounding" and pressuring her not to prosecute Montreal-based SNC-Lavalin company.
"I experienced a consistent and sustained effort by many people within the government to seek to politically interfere in the exercise of prosecutorial discretion, in an inappropriate effort to secure a deferred prosecution agreement with SNC-Lavalin," ex-minister Jody Wilson-Raybould told the House of Commons.
Wilson-Raybould added that she received "veiled threats" from Michael Wernick, Canada's top bureaucrat, that "a collision with the prime minister on these matters should be avoided."
Trudeau responded that he "completely disagrees with the former attorney general's characterization of events."
The lawmakers are due to hold an emergency debate on the scandal on Thursday.
Firm bribed Gadhafi government
The scandal has rocked the Trudeau administration as the Liberal party leader prepares to run for re-election in October. It centers around allegations that SNC-Lavalin bribed officials in the Libyan government under strongman Muammar Gadhafi between 2001 and 2011.
The company was formally charged with corruption in 2015, with prosecutors saying that it had paid Gadhafi's regime 130 million Canadian dollars (US$99 million) for lucrative government contracts, including the Great Man-Made River Project, the biggest irrigation project in history.
SNC-Lavalin heavily lobbied the government to settle the corruption case out of court. The firm has repeatedly claimed that anyone responsible for the wrongdoing has since left the company.
'Serious red flags'
Wilson-Raybould testified that "the prime minister asked me to help out, to find a solution for SNC, citing that if there is no DPA (deferred prosecution agreement), there would be many jobs lost and that SNC would move from Montreal."
Jody Wilson-Raybould she was "barraged" and faced "hounding" over the case
She said 11 other top officials, including Finance Minister Bill Morneau, raised concerns that the firm would move to London if it did not face favorable legal conditions in Canada.
They "urged me to take partisan political considerations into account, which was clearly improper," she said, adding that while "not illegal," it had "raised serious red flags."
Wilson-Raybould resigned in January, along with Trudeau's longtime ally and principal secretary Gerry Butts, who has been vague about his reasons for leaving the government.
Freeland closes ranks with Trudeau
Conservative Party leader Andrew Scheer said that the prime minister should step down over the scandal, claiming Trudeau "can no longer and in good standing with a clear conscience lead this nation." He also called for a federal investigation into the possibility that government officials obstructed justice.
"The matter at hand appears, on its face, to be a gross violation of the law," Scheer wrote in a letter to federal police.
Trudeau disputed the nature of the discussions in a news conference, saying that "our government will always focus on jobs" and that his administration was merely debating the impact the case could have on the company's Montreal workforce.
In an unusual move, Foreign Minister Chrystia Freeland appeared at Canada's CBC broadcaster to pledge her full support to the 47-year-old prime minister.
"Of course I support the prime minister 100 percent," said the popular minister, whom some see as a possible successor of Trudeau.
"I am very clearly of the view that the prime minister would never apply improper pressure," she added.
es/jil (AFP, Reuters)
Canadian PM fires ambassador to China over Huawei comments
Prime Minister Justin Trudeau has fired Canada's envoy to China. Ambassador John McCallum had said it would be "great" if the US dropped its extradition request for a top Huawei executive arrested in Vancouver. (27.01.2019)
Trudeau sorry for 'historic wrong' against aboriginal Canadians
The prime minister has apologized to First Nations people in the province of Newfoundland and Labrador for abuse at assimilation-oriented schools. The system of boarding schools operated until 1980. (25.11.2017)
Canada legalizes recreational marijuana use
Canada's Senate has passed a landmark law, known as the Cannabis Act, legalizing recreational marijuana use. Canadians will have to wait until September at the earliest, however, before they can buy the drug legally. (20.06.2018)
Related Subjects Libya, Canada
Keywords Justin Trudeau, SNC-Lavalin, Libya, Jody Wilson-Raybould, Canada, corruption, bribery
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The lazy days of summer may include sleeping late, deviating from structure and routine, and enjoying warm weather activities. Unfortunately, once the school year has wrapped up those leisurely days can also lead to summer brain drain.
In fact, research indicates that all of the downtime over the summer months can lead to a month or more worth of academic regression that teens need to compensate for once the new school year begins. Fortunately, with a minimal amount of deliberate planning you can ensure that your teen has a fun-filled summer that is also enriching and engaging.
• Balance Downtime with Engagement – Allow for a deviation from the typical, hectic school year schedule. This might mean allowing your teen to sleep later than his or her school day wake up call, but it doesn't mean sleeping the day away. Compromise with your teen about reasonable times to go to bed at night and start the day in the morning. Consider maintaining some type of healthy sleep cycle routine while consenting to slightly later bedtimes and wake up times.
When planning for an enriching summer, parents needn't reserve a spot in a two month long camp or a full time summer school program.
A variety of one-day or short term activities can allow for a teen to experience an assortment of interests while still enjoying some summer relaxation. When creating a summer calendar, discuss your teen's interests with him or her and find opportunities for exploration. If your teen wants to learn more about sailing, consider a sailing lesson, pick up a few books about sailing, or attend a local sailing competition.
You could also encourage your teen to take a high interest course such as Photography or Forensics. Additionally, consider seeking math or reading programs that meet for one or two days per week rather than every day, so that teens are optimally engaged for a shorter period and also have time to explore other interests, as well.
• Implement Mini Brain Workouts – In addition to more formal camps or clinics, build in mini brain workouts to keep your teen from experiencing summer brain drain. These activities could include crossword puzzles, creating a grocery list that remains within a set budget or even assisting with doubling or tripling a recipe for a family barbeque. These activities should be informal and fun!
• Encourage Physical Exercise – Physical exercise promotes the flow of oxygen to the body and brain and helps teens to reduce stress. The warmer summer weather allows a perfect opportunity for playing a game of basketball, taking a walk or going for a swim.
• Promote Service Learning – Help your teen find a way to give back to the community this summer. Whether it be volunteering at a soup kitchen, helping with a community cleanup project or assisting with story hour for smaller children at a local library, community service opportunities will keep your teen engaged and also help him or her to understand the power of helping others.
• Limit Screen Time – Rather than battling with your teen about the amount of time they are spending playing video games, texting or using social media, sit down and discuss the parameters up front. Making your teen a part of the conversation and setting reasonable limits for device usage at the start of the summer vacation will ensure that everyone understands the terms up front. Setting boundaries in advance will prevent discussions about device use from being a part of your daily interactions with your teen this summer. Also, consider creating a list of tasks such as reading or taking a walk which need to be completed before screen time is an option.
Summer should allow plenty of opportunities for carefree days spent with friends and family, but with just a bit of planning the summer months can be an incredible opportunity for growth and exploration.
Jennifer Walsh-Rurak, Ed.D. earned her doctorate in Educational Leadership from Northeastern University. Dr. Walsh-Rurak is a regional manager and school leader at Fusion Academy. Fusion utilizes a one-to- one instructional model to customize and individualize instruction to meet the needs of a variety of learners. Additionally, Fusion offers over 450 courses providing a multitude of opportunities to promote an enriching and meaningful summer.


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Update on Nicaragua
Journeys to Nicaragua are on the 2019 calendar for Anderson Mill Road Baptist Church's Missions outreach after cancellations this year due to civil unrest and violence.
The Mill is sponsoring trips to the Central American country in the spring and summer as the dangers have waned. The trouble in Nicaragua began on April 18 with protests in several cities against reforms by President Daniel Ortega that raised social security taxes while decreasing benefits. Around 30 people were killed in the first five days and more than 300 since then, according to the Inter-American Commission on Human Rights.
The Mill will send a group of about 20 to the Pearl Foundation's mission in Granada from April 30-May 6, while another contingent will travel there in the summer, said Darrell Hinson, a member of The Mill, who with his wife Linda founded Pearl Foundation in 2007 after making numerous mission trips to Nicaragua. A group of 20 to 30 from The Mill will travel to Chosen Children's site in Masaya from July 13-20, said Darrell Cothran, assistant director of Chosen Children Ministries and The Mill's media Pastor.
"It just wasn't safe for us to send teams to Nicaragua this year," said Jason Williamson, The Mill's Missions Pastor. "We're going to trust our partners in the field. When they say it's not safe to come, we listen."
Missions in Nicaragua typically attract families with children because the travel is relatively short – with good flight connections from Greenville-Spartanburg International Airport – and good accommodations in the field. For those reasons, Nicaraguan trips are often the first that a person or family will take.
The Mill wasn't alone in pulling out of missions to Nicaragua. Numerous trips sponsored by Evangelical churches or groups from the United States were postponed or canceled during the spring and summer, Christianity Today said, leaving people they served in worse shape amid the national crisis. And the Church of Jesus Christ of Latter-Day Saints pulled more than 350 missionaries from Nicaragua in June, The Salt Lake Tribune reported.
At the same time, Catholic churches were on the front lines of the protests, according to the Wall Street Journal, with clergy assaulted and numerous churches "attacked, shot at, looted or defiled," primarily by "government-allied paramilitary groups."
About half of Nicaragua's believers are Roman Catholics, while more than a third are affiliated with Evangelical churches, according to the Central Intelligence Agency's Factbook. Nicaragua is the largest country in Central America, with its population (6.025 million) about a million more than South Carolina's and its land mass about a third larger than the Palmetto State.
While many mission teams work in regions that weren't directly impacted by the violence and protests, one critical issue was getting there, since most teams flew into the major cities of Managua or Granada and then traveled by bus for several hours to the sites of their mission work.
Cothran said that protestors frequently blocked roads from the big cities to the outposts, creating dangerous situations for Americans on mission trips.
The Hinsons were scheduled to return to Nicaragua on May 30, but by then, Darrell Hinson said, "the unrest had escalated to mass killings, looting and burning of buildings. We had to cancel our trip and subsequently cancel team trips scheduled for the summer." Six mission trips, comprised of more than a hundred people, were scrubbed, he said.
"Fortunately we have a wonderful staff of Nicaraguans that carry on the work of the ministry in our absence," Hinson said. "One of the main activities of our ministry is the preparing and feeding a meal each day to the children in a barrio called Pantanal. Before the civil unrest, we were feeding 80 to 90 children per day.
"We are now averaging 200 children per day. The reason for the increase is a tremendous increase in unemployment. The area we serve is dependent on tourism for many of its jobs. Since the trouble began tourists stopped coming and many hotels, restaurants and other tourist-related businesses closed, putting thousands out of work."
Even before the trouble, the situation in Nicaragua was dire, Williamson said.
"In some places, it's a very hard life with not a lot of opportunities," he said, recalling a time when he preached to a group of Nicaraguans at a garbage dump. It was a place where many went to scavenge for discarded clothing, appliances and the like.
Cothran said that Nicaragua is "the second poorest country in the region, right down there with Haiti. You kind of have two classes of people down there. The wealthy live in the biggest cities, while five miles outside of town you find the poorest of the poor."
Cothran said that unemployment in the area that Chosen Children Ministries serves was running about 35 percent before the trouble started. Now, he said, joblessness is 65 percent.
"For those who are working, salaries are running about $2 a day," he said.
Chosen Children provides meals and other aid, drills wells, plants churches, and partners to provide economic development to the area it serves, among other things.
Pearl Foundation has a feeding program and sponsors backyard Bible clubs for children, discipleship classes, sports, prison and nursing home ministries.
If you would like to be a part of one of the trips and make a difference in Nicaragua, please contact Keri, our Missions Logistic Coordinator at keri@amrbc.org.
Posted in Mission Stories
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Interning in Uganda with Benjamin House
For as long as I can remember, my mom and dad have been faithful about a calling to child sponsorship. As my brother and I grew up, we were able to write letters to a child all the way across the world who was close to our age. We talked to him about sports, school,…
Reflections upon "Serve the 'burg"
"But you will receive power when the Holy Spirit has come upon you, and you will be my witnesses in Jerusalem and all Judea and Samaria, and to the end of the earth." Acts 1:8by Casey Seaman
The Laneys' Story: A Family Changed by Missions
God changed Brandon and Summer Laney's lives and family forever in 2011 when He led them to the village of Najjanankumbi in Uganda, Africa. The trip was not on their agenda for that year, and it was not something they had previously considered. However, God had big plans for not only Brandon and Summer, but for their children also. They have returned to Uganda almost every year since 2011, and two of their children have jumped on board as well.
Lost and Found An Emerging Hispanic Ministry
For Ricky Maxwell, his journey with a new ministry opportunity began one morning during quiet time with the Lord. Shortly after reading scripture and praying, Ricky felt compelled to contact his friend Mark Bennett, a Mill member and missionary in Mexico. "The Lord laid on my heart that I needed to look into a Hispanic ministry in Spartanburg, so I called Mark right then and there," Ricky said. This conversation allowed him to discover a unique opportunity that he says he "never saw coming.
He Is Enough
"And let us not grow wearing of doing good, for in due season we will reap, if we do not give up." (Galatians 6:9, ESV) When Drake O'Sullivan was born, he was perfectly healthy. Drake passed all newborn tests with high scores and within 24 hours, he was released to go home with his parents.…
Journeys to Nicaragua are on the 2019 calendar for Anderson Mill Road Baptist Church's Missions outreach after cancellations this year due to civil unrest and violence. The Mill is sponsoring trips to the Central American country in the spring and summer as the dangers have waned. The trouble in Nicaragua began on April 18 with…
Disaster Relief at The Mill
On August 25, 2017, Hurricane Harvey made its destructive landfall in Texas as a category four hurricane. Chris Bennett, a member of The Mill, felt called to action. He travelled to Houston with his boat in tow, ready to assist those who were stranded and in desperation due to the rising floodwaters in the aftermath…
Brandon Laney's Story
The Mill has recently formed a new ministry within our missions efforts to address disaster relief. We have partnered with the Southern Baptist Convention Disaster Relief organization. I saw a Facebook post from The Mill on Mission saying that there was a GroupMe being setup for Disaster Relief in preparation for Hurricane Florence. God told…


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Make the wild boar a tourist attraction say wildlife fans
The animals have been the subject of much debate in the Forest of Dean over the years
A family of boar in the Forest of Dean (Image: Adrian Worrall)
Wild boar should be marketed for tourism, according to a group who wants to see an end to the yearly cull.
Forest of Dean Wild Boar Cull Saboteurs suggest that the best way to manage the animals is a bylaw prohibiting people feeding them.
As the area is the only place where the boar can be seen in their natural habitat, the group believes they could bring more people to the area.
Survey figures estimated there were 1,562 feral wild boar roaming the Forest last year and populations were spreading to new areas.
That is an increase of more than 500 on the year before.
The target population for the Forestry Commission is 400 and the annual cull helps to bring numbers under control.
Teenager's diet of cooked breakfasts, sausages and waffles is down rare disorder which affects just 100 people in the world
But Forest of Dean Wild Boar Cull Saboteurs said: "The boar, if left alone, will find a natural balance.
"What is needed is education, a bylaw prohibiting the feeding of the boar, teaching people how to live with them.
"And surely these animals can be marketed, the dean is the only area where wild boar can be seen in their natural habitat, that must be a boon for tourism.
How should the numbers of wild boar be controlled?
The group added: "While we will continue to oppose any cull of these creatures we will happily work with any agency to promote coexistence with this welcome return to the British countryside."
Accidental and deliberate releases from wild boar farms has let to populations being re-established, after they were hunted to extinction in the 17th century.
Police release images of two men they want to speak to in connection with a burglary
Gloucestershire Live reported last month that Lynx could be released to help the situation.
A trial at Kielder Forest using the natural predators is expected to show how it can reduce numbers naturally, without doing it en masse.
However, NFU countryside adviser Claire Robinson said that may be a risky operation.
"The biggest concern we have would be the impact on farm animals with lynx preying on lambs, poultry and outdoor piglets – those animals are farmers' livelihoods," she said.
Forest Green Rovers FC"It was a little bit farcical" – Forest Green Rovers boss Rob Edwards on Mansfield Town abandonmentForest Green Rovers 0 Mansfield Town 0 (match abandoned after four minutes)


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Home Biography Michael Jordan Bio, Age, Height, Net Worth, University
Michael Jordan Bio, Age, Height, Net Worth, University
Vaib Sharda
Michael Jordan (born February 17, 1963), also known as MJ. He is a former professional basketball player and an American businessman. He is the principal owner and manager of the Charlotte Hornets of the National Basketball Association and 23XI Racing in the NASCAR Cup Series.
A must read: Michael Jackson death, bio, age, height, family, wiki.
Michael Jordan Bio
Known as : Michael Jordan
Profession: Professional basketball player and businessman
Guy: 58 years old
Date of birth: 17 February 1963
Birthplace: Brooklyn, New York, USA.
Birthmark: Aquarius
Length: 198 cm (6 feet 6 inches)
Weight: 98 kg (216 lbs)
Body dimensions: 44-36-40
Net worth: $1.6 billion
Salary: To be revised.
Name of the parents: Michael Jeffrey Jordan
Alias : M.J., His Eminence, Air Jordan, G.O.A.T.
Religion : Roman Catholic
Sexual orientation: Direct
Body shape: Direct
Shoe size: 13 (USA)
Eye color : Brown
School: Emsley A. Laney High School
College: University of North Carolina
Brother(s) : Larry Jordan, James R. Jordan JR,
Sister(s) : Deloris, Roslin.
Marital status: Married with
Husband: Yvette Prieto, Juanita Vanoy (1989-2002)
Relationship with : Vanessa Williams, Loredana Jolie, Juanita Jordan, Carla Knafel, Kylie Ireland, Nicole Mitchell Murphy, Yvette Prieto.
Children: The twin girls are named Victoria and Isabel.
Jordan was born on the 17th. Born Feb. 1963 in Brooklyn, New York, the daughter of Delores, who worked for banks, and James R. Jordan, Sr.
His family moved to Wilmington, North Carolina, when he was a small child. Jordan was the fourth of five children. He has two brothers, Larry Jordan and James R. Jordan Jr. and an older sister, Delores, and a younger sister, Roslyn. Jordan's brother, James, retired in 2006 as a staff sergeant with the 35th Signal Brigade, XVIII Airborne Corps of the U.S. Army.
He played his 15th season in the National Basketball Association. For the Chicago Bulls and Washington Wizards. His bio on the NBA website reads: (Side note, Jordan is the greatest basketball player of all time).
He was one of the most promotional athletes of his generation and was considered important to the NBA's worldwide broadcast from 1980 to 1990.
He left North Carolina a year before his expected graduation date to enroll in 1984. NBA Draft, he returned to North Carolina to graduate in 1986.
He married Juanita-Vana in 1989 and they have two sons and a daughter. The wires… Jeffrey Michael, Marcus James. The girl… Jasmine. Jordan and Vanoy filed on the 4th. They filed for divorce on 1 January 2002, due to irreconcilable differences, but reconciled soon after.
He asked his former girlfriend, Cuban-American model Yvette Prieto, to marry him on Christmas 2011, and they married on the 27th. April 2013 at Bethesda Episcopal Church. The 30th. In November 2013, it was announced that they were expecting their first child. On the eleventh. In February 2014, Prieto gave birth to two identical twin girls named Victoria and Isabel.
Also read : Vicky Macaulay Culkin, biology, age, height, net worth, facts.
Age, height and dimensions
Michael Jordan is 58 years old. Michael Jordan is 198 cm tall and weighs 98 kg. Size 44-36-40 and zodiac sign Aquarius.
He is very popular and active on social media. His Instagram account has 21.7 million followers and his Twitter account has 4.1 million followers.
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The Flip-Flop block has aluminum hardcoat-anodized side plates and features Hard Lube-anodized aluminum sheaves for strength and corrosion resistance.
The high-load flip-flop blocks pivot around the line axis to keep line close to the deck. Hinged construction allows variable leads. Lockoff provides a temporary stop to free up winches.


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Tokolo Asao
野老朝雄
Geometry, Connection, Harmony
Architecture & Design Sport & Pastimes Visual Arts
Photo by Tsuruoka Shintaro
Tokolo Asao is an interdisciplinary artist, designer and educator whose work came to international attention when his graphic artwork Harmonised Chequered Emblem was selected to represent the Tokyo 2020 Olympic and Paralympic Games.
Tokolo is also a trained architect and a graduate of Tokyo Zokei University. He established a connection to London when he studied at the Architectural Association School of Architecture (AA) under the artist and architect Egashira Shin, with whom he undertook an apprenticeship before founding his own studio in 2001.
Notable works and collaborations
Tokolo's mastery of numerous and diverse subjects, including mathematics, architecture, design, fashion and art, is reflected in the interdisciplinary nature of his practice. His various works and collaborations include carpet design for United Cinemas in Maebashi in 2007, Issey Miyake's Bao Bao range of bags in 2008 and 2015 and three-dimensional façades for buildings such as F-town Building in Sendai in 2007 and the Education Center at Kogakuin University in 2012. One of his most popular product designs is the Tokolo Pattern Magnet which uses the Japanese karakusa (lit. 'Chinese grass') pattern. The square and triangular magnet tiles can be used individually or joined together to create endless design possibilities. The magnet was selected to be part of the Japanesque Modern Collection, a Japanese government-supported selection of innovative Japanese products, in 2006. In 2016, Tokolo began working with ceramics for the first time in the famous ceramics town of Arita in Saga Prefecture, incorporating his designs into dishes and tiles.
'TOKOLO PATTERN' for BAO BAO ISSEY MIYAKE | Photo by Yamamoto Ikunori
Close-up of the BAO BAO bag by Issey Miyake with patterns designed by Tokolo Asao. Photo by Kimura Choku
FRP F-town Building (Architect: Atelier Hitoshi Abe), Facade pattern design by Tokolo Asao, Miyagi, 2007 Photo by Ano Daici
Close-up of the patterned facade of the F-town Building (Architect: Atelier Hitoshi Abe), Miyagi, 2007 Photo by Ano Daici
PPP Tokolo Pattern Magnet (produced by Kami No Kousakujo), 2019 Photo by Hiraga Tetsu
PPP Tokolo Pattern Magnet (produced by Kami No Kousakujo), 2019 Photo by healthy
Tokyo 2020 Olympic and Paralympic emblems
In 2016, Tokolo's artwork titled Harmonised Chequered Emblem was unveiled as the winning design for the Tokyo 2020 Olympic and Paralympic emblems out of 14,599 entries submitted to a public competition. The design is composed of a connecting sequence of three types of rectangular shapes that form the tessellated circular and U-shaped patterns of the Olympic and Paralympic emblems. The three varieties of rectangular shapes represent different nationalities, cultures and ways of thinking coming together, conveying the message of "Unity in Diversity". Tokolo created both emblems to be of the same size and volume – each is made up of a total of 45 rectangles – as an expression of equality. The design makes elegant and subtle references to Japanese traditions: the historical chequerboard pattern, ichimatsu moyо̄, was popular in Edo-period Japan (1603-1867 CE), while the use of the vivid indigo blue, ai, alludes to Japan's history of indigo dye production.
Sketches of the Tokyo 2020 Olympic and Paralympic Games emblems, designed by Tokolo Asao. Image: Tokolo Asao 2019
The emblem was featured in the Tokyo 2020 Olympics Opening Ceremony, in a drone light show above the Olympic Stadium, on 23 July 2021, and demonstrated the geometric varieties inherent in the design with the movement of its rectangles.
Themes and Processes
Tokolo has been creating work that explores the theme of tsunageru, 'to connect', since being moved by the tragic events of 11 September 2001 in the United States. By connecting different elements such as simple geometric shapes and curved lines into patterns, he aims to reflect the harmony he wishes to see in the world. Though many of his works are devised using mathematical logic, they can be re-created using just a compass and a ruler. The resulting designs are translated into versatile two-dimensional and three-dimensional works of art, design and architecture in a variety of media including ceramics, urushi (lacquer), woodwork, Edo kiriko cut glass and canvas prints, many created in collaboration with expert Japanese craftspeople. In more recent works, Tokolo has also been experimenting with the rich range of shades of the colour ai (Japanese indigo) also known as 'Japan blue'.
Tokolo Asao at work in his studio. Photo by Tsuruoka Shintaro
Tokolo Asao's work with ceramics
In 2016, Tokolo was commissioned to design his first ever ceramic dishes, using a medium he had not worked with before. The commission was followed by an exhibition proposal from the Kyushu Ceramic Museum. Tokolo was invited to explore new possibilities for Arita ceramics made in the town of Arita, where porcelain was first produced in Japan over 400 years ago. The artist worked with local potters to produce new works with a particular focus on the colour blue, which characterized early Arita ware until mid-17th century CE. With these potters, Tokolo mixed glazes containing various concentration levels of cobalt, producing dishes and tiles that demonstrate a vast range of shades of blue. The artist also experimented with centrifugal force to apply decoration. The exhibition [ ARITA X TOKOLO ] was shown at the Kyushu Ceramic Museum in the autumn of 2019.
Centrifugal Force Pattern Dishes by Tokolo Asao. Photo by Ishimaru Hiroshi
Form/Void Tiles by Tokolo Asao. Photo by Ishimaru Hiroshi.
Aritayaki Ruri 100 Steps Small Dishes, Installation view of [ARITA x TOKOLO] exhibition, 2019. Photo by Ishimaru Hiroshi
Exhibition at Japan House London
Over the past 20 years, Tokolo has held teaching positions in subjects as diverse as fashion and architecture at the prestigious Musashino Arts University, Kuwasawa Design School, University of Tokyo and Tokyo Zokei University. His work has been exhibited in many high-profile art venues around Japan including 21_21 Design Sight in 2015, Aomori Contemporary Art Centre in 2016 and The Kyushu Ceramic Museum in 2019. A sample of Tokolo's work was on display across all three floors at Japan House London in 2021, as well as a creative street crossing on Kensington High Street specially designed by the artist. The selection of works included 100 patterns printed on canvas on the Lower Ground Floor, an original Tokyo 2020 art poster, ceramics such as tiles, dishes, unusual decahedron cups, and laser-cut wood works presented on the Ground Floor. You can browse the virtual exhibition on our website now.
The exhibition 'Tokolo Asao [CONNECT] Individual and Group' was on at Japan House London
Tokolo Pattern 100 Works (2020) was presented on the Lower Ground Floor at Japan House London
A variety of works by Tokolo Asao, such as laser-cut wood works were presented at Japan House London
Visitors to the exhibition could see Tokolo Asao's recent work 'One in a Thousand Cranes Higashi Matsushima' (2020), created in collaboration with Tsuruoka Shintarō and Odaira Yūko of COMU LLC. The work preserved some of the paper cranes that were sent to Higashi Matsushima in Miyagi Prefecture as a symbol of hope following the Great East Japan Earthquake and tsunami in 2011.
A number of products designed by Tokolo Asao were available in The Shop at Japan House London
Creative street crossing on Kensington High Street designed by Tokolo Asao
Virtual Exhibitions | Tokolo Asao [Connect]


The specific trend that I'm identifying is a melding of the environmental character of the home and the workplace. There will be a desire for a more residential, less corporate feeling at the office. Not only the look and feel, but amenities you might find in your home will be included in the office such as exercise equipment, kitchen and gaming, and less formal meeting places. This reflects a merging of market types from hospitality, to corporate, residential, retail, and even healthcare in office design.
Over the past few years we've seen a steady surge of technology becoming yet another tool in our designer toolbox. No longer left solely to the electrical engineer, designers are playing with technology in new ways every day. We predict that 2016 will be the year of interactive digital elements in hotel design, from light panels that mimic your shadow as you walk past, to touch integrated bar tops that allow the customer to re-order their favorite drink. The limits are dropping away in terms of how people interact with spaces and as designers we are ready to make that move with the masses.
This trend sketch "crystal ball moment," is dedicated to an incredible material: fish leather. Arcsine recently specified a textured leather for a bar countertop, and since then my eyes have been looking for new ways to work with leather and new leather options. During a recent trip to Iceland, I had the opportunity to visit one of the few fish tanneries in the world, Atlantic Leather. This incredible group of people in the small northern town of Sauðárkrókur divert fish skin from landfills and transform it to a luxury material. Currently, the material is used most often in the fashion industries for clothing, accessories, jewelry, and shoes. However, the design community is starting to take notice. The smooth, dark spotted pattern from the deep-sea wolffish is my personal favorite; though the texture of the perch leather is bold and inviting to the touch. Hundreds of finishing options are also available in colors, metallics, and sheens. This is a building material that can be used in its natural tone, or dressed up for an array of exciting applications.


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Texas, the SEC, and the Value of a Top Recruit
By DawgOutWest Jul 27, 2021, 6:09pm EDT
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Photo by George Walker/Icon Sportswire via Getty Images
Yesterday, multiple high-level University of Texas sources told me that UT Board of Regents Chairman Kevin Eltife wants to see the Longhorns in the SEC for the 2022 season.
What about the small matter of the $150 million dollar buyout that Texas and OU have to pay to the Big 12 if they leave before 2025? Well, they made it clear that Eltife had a plan.
"He believes getting into the league for the 2022 season would help Texas from a recruiting and branding standpoint, and quicken the university's ascent back to the top of the sport."
It now looks like that sum could come from the remaining dollars on the Longhorn Network contract that Texas made with ESPN a decade ago, but the sources were clear that the money wasn't nearly as important to UT brass as getting the program back to the top of the college football landscape.
Since the start of the CFP era, Texas's recruiting has been all over the map. Tom Herman signed back-to-back top five classes in 2018 and 2019, but the Longhorns have mostly recruited on a level a tier or two below elite since 2014. In a state with as much FBS talent as Texas, that's unacceptable.
In 2020, UT signed three of the top 10 players in Texas, but half of the top thirteen prospects in the state headed to the SEC. Go back another year to 2019 and you'll see that only three of the top 20 players in the state decided they wanted to play their college ball in Austin. To make matters worse, hated Texas A&M signed six of the top 13 players in the Lone Star State.
Go look at the top players in Texas in the class of 2021. The #2 player in the state, Ja'Tavion Sanders, went to UT. After him, you have to scroll all the way down to the 26th rated player in the state to find the next player in the class who decided to become a Longhorn. Yes, 2021 featured a staff turnover at Texas and a pandemic, but it's still jarring to look at. Eleven of the top twenty players in Texas went to SEC schools.
Recruiting at Texas has been inconsistent, and players are leaving to go play at Clemson, Ohio State and the SEC. The power brokers have been growing restless, and the straw that broke the camel's back may have come in the form of Quinn Ewers.
Ewers is the nation's #1 prospect for 2022, and he's the type of quarterback talent that is an absolute necessity if you want to compete for championships in this era of college football. After once being committed to UT, Ewers decommitted from Texas in October of last year. He's heading north to play his football at Ohio State.
Don't be mistaken, watching prospects like him play their college ball at places other than Texas is part of the reason why UT no longer sees membership in the Big 12 as a viable option.
My sources at Texas have made one thing very clear this week about Eltife, and that's that he is much more than a casual fan. "He follows recruiting like you and me," said one source.
It has been made clear to me many times over the last week that Eltfie knows SEC membership will help the Longhorns on the trail. The quicker the UT staff can pitch future home games against teams like Alabama, Georgia, LSU and Florida, the better. Oh, and there's also the small matter of the rivalry with Texas A&M.
The next QB prospect on the level of Quinn Ewers is a guy by the name of Arch Manning. He's the latest in the line of passers that includes his grandfather Arch and his uncles Peyton and Eli.
He will be the most hyped recruit in the history of college football, and insiders say he's interested in playing at Texas. The problem is that he's also interested in continuing the family legacy of playing in the SEC.
Texas would love to sell him on the ability to both play in the Southeastern Conference and for the flagship university of the Lone Star State, which begs a bit of an interesting question. Is a sixteen year-old quarterback in New Orleans and other highly rated prospects like him at least partially responsible for UT's willingness to shell out $150 million dollars?
By all accounts, Eltife understands modern college football, and that means he understands what entering the SEC with a Manning under center would mean to the program.
Sure, there's a lot of other factors that Texas has taken into account as they've navigated this move. But make no mistake, Arch Manning, and many other highly rated prospects just like him are watching what Texas is doing… the Longhorns are making sure of it.


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\section{Introduction}
\label{sec:intro}

It is well accepted that active galactic nuclei (AGN) are powered by the accretion of matter onto a supermassive black hole (SMBH) through a geometrically thin, optically thick disk \citep[e.g.,][]{Shak73}. The ``unified model'' of AGN \citep{Antonucci93, Netzer15} hypothesizes the presence of a dusty circumnuclear torus at the parsec scale, explaining the dichotomy between type-1 and type-2 AGN through different viewing angles. The actual morphology and composition of this material is an open question, although several works suggest a clumpy distribution of optically-thick clouds rather than a homogeneous structure \citep[e.g.,][]{Honig07, Risaliti07, Balokovic14, Marinucci16}.

A significant fraction ($\sim 10-25 \%$) of the AGN population, in the local Universe, is theoretically expected to be obscured by Compton-thick (CT) material (with an equivalent neutral hydrogen column density, $N_{\rm H} \gtrsim 1.5 \times 10^{24}\,\rm cm^{-2} $) in order to explain the observed peak of the cosmic X-ray background (CXB) in the 20-50~keV band \citep[see e.g.,][and references therein]{Ueda14}. However, the observed fraction of CTAGN is much smaller than these values. Only about $8\%$ of the AGN in the {\it Swift}/BAT 70-month catalog are found to be CT \citep[see][]{Ricci15}. The major difficulty in identifying CTAGN is due to the fact that the emission in the soft X-rays, ultraviolet (UV), and optical, which is directly produced by the AGN, is heavily attenuated due to obscuration. The only two spectral bands where the obscuring material is optically thin up to high column densities are the hard X-rays ($\gtrsim 15$~keV) and the mid-infrared ($5-50\,\rm \mu m$). Thanks to its unprecedented sensitivity covering the $3-79$~keV band, \textit{NuSTAR} is playing a key role in identifying the missing fraction of CTAGN and determining their properties \citep[e.g.,][]{Koss16, Marchesi18}.

In this paper, we present multi-epoch observations of the Seyfert-2 galaxy NGC 5347 ($z=0.00792,\, D =35.5 \rm ~Mpc $) using the \textit{Chandra X-ray Observatory}, \textit{Suzaku}, and \textit{NuSTAR}. This source is part of a \textit{NuSTAR} Legacy Survey (PI: J. M. Miller) aiming to study an optically-selected volume-limited sample of 22 Seyfert-2 galaxies that were identified in the CfA Redshift Survey \citep{Huchra83}. \cite{Risaliti99} classified this source as a CTAGN ($N_{\rm H} > 10^{24}\,\rm cm^{-2}$) on the basis of its large Fe K$\alpha$ equivalent width ($\rm EW > 1.9~\rm keV$) measured in an \textit{ASCA} spectrum. However, \cite{Lamassa11} classified the source as Compton thin, with $N_{\rm H} = 5.6_{-2.3}^{+3.2}\times 10^{23}~\rm cm^{-2}$, based on the \textit{Chandra} spectrum. We note that this source is a megamaser galaxy showing strong [\ion{O}{4}] emission, negligible star formation and no hint of silicate absorption at 10~$\rm \mu m$ \citep{Hernan15}. The paper is organized in the following way: in Section \ref{sec:sdss} we present the analysis of an optical spectrum of the source. The X-ray observations are presented in Section \ref{sec:reduction}. We discuss the X-ray spectral fitting within the context of various models in Section \ref{sec:spectral_fits}. Finally, in Section \ref{sec:discussion} we discuss the implications of our results and we present spectral simulations of this source for the future high-resolution observatories: {\it XRISM} and {\it Athena}. The following cosmological parameters are assumed: $\Omega_{\rm M}= 0.27$, $\Omega_{\Lambda} =0.73$ and $H_0 = 70\,\rm km s^{-1}\rm Mpc^{-1}$.

\section{Optical spectroscopy}
\label{sec:sdss}

NGC~5347 was observed as part of the Sloan Digital Sky Survey (SDSS) on 2007-01-15 with a 3$''$ (513 pc) diameter fiber for a total exposure of 4203 seconds \citep{SDSSDR7}. The continuum and the absorption features were fit using the penalized PiXel Fitting software \citep[{\tt pPXF};][]{Cappellari04} to measure a central velocity dispersion for the galaxy. A stellar template library from VLT/Xshooter \citep{Chen14} was used with to fit the spectrum with optimal stellar templates following the general procedure in \cite{Koss17}. These templates have been observed at higher spectral resolution ($R=10,000$) than the AGN observations and are convolved in {\tt pPXF} to the spectral resolution of each observation before fitting. When fitting the stellar templates, all the prominent emission lines were masked (see upper panel of Fig.~\ref{fig:sdss}).

\begin{figure}
\centering

\includegraphics[width = 1.\linewidth]{ppxf_spectra.pdf}
\includegraphics[width = 1.\linewidth]{optical_spectra.pdf}

\caption{SDSS spectrum of NGC~5347 (black solid lines) and the best-fit models (red dash-dotted lines). The upper panel shows the spectrum of NGC~5347 with the fits of the absorption lines in the \ifmmode \left[{\rm Ca H+K}\,\textsc{ii}\right\,\lambda3935,3968 \else Ca H+K$\,\lambda3935,3968$\fi, \ifmmode \left{\rm Mg}\,\textsc{i}\right\,\lambda5175 \else Mg\,{\sc i}\,$\lambda5175$\fi\, and the \caii\ triplet spectral spectral regions. The grey shaded areas represent the regions with emission lines which are excluded from the fit (e.g., Ca H$\lambda$3968.47 and [\ion{N}{1}]$\lambda$5200, [\ion{Fe}{2}]$\lambda$8619). The bottom panel shows the rest frame NGC~5347 spectra corrected for Galactic extinction in the \Halpha\ and the \Hbeta\ complexes.}
\label{fig:sdss}
\end{figure}

The main aim of studying the SDSS spectrum of this source is to determine the mass of the SMBH from the stellar velocity dispersion using a high-resolution spectrum. In fact, it has been shown that, for some cases, low-resolution spectra could lead to an overesitmate of the velocity dispersion \citep[e.g.,][]{Brightman18}. In the case of NGC 5347, we find a velocity dispersion of $89\pm3~\rm km~s^{-1}$ in the \ifmmode \left[{\rm Ca H+K}\,\textsc{ii}\right\,\lambda3935,3968 \else Ca H+K$\,\lambda3935,3968$\fi\ and \ifmmode \left{\rm Mg}\,\textsc{i}\right\,\lambda5175 \else Mg\,{\sc i}\,$\lambda5175$\fi\ regions (3830-5600~\AA) and $93\pm5~\rm km~s^{-1}$ for the \caii\ triplet spectral region (8350--8700\,\AA) for a weighted average of $90 \pm 3~\rm km~s^{-1}$. This measurement is consistent with the literature values \citep[$73\pm14 ~\rm km~s^{-1}$, $103 \pm 10 ~\rm km~s^{-1}$;][respectively]{Terlevich90,Nelson95} but  shows significantly less error. Using the \cite{Kormendy13} relation, this velocity dispersion implies a black hole mass of $\log\left( M_{\rm BH}/M_{\odot} \right) = 6.97 \pm 0.13$. This value is consistent with the measurement reported by \cite{Izumi16}, $\log \left( M_{\rm BH}/M_{\odot} \right) = 6.73 \pm 0.55$, from the velocity dispersion measurements above

\begin{table}
\centering

\caption{Measured emission-line fluxes, Gaussian amplitude over noise, and EW for the major emission lines observed in the SDSS spectrum of NGC~5347. }

\begin{tabular}{llll}
\hline \hline
Line	&	Flux	&	A/N	&	EW \\
 & $(10^{17}~\rm erg~s^{-1}~cm^{-2})$ & & (\AA) \\ \hline

\ion{He}{2}$\lambda$4686 & $  217.59 \pm 2.06$ & 11.25 & 1.32 \\
\Hbeta & $650.68 \pm 5.77$ & 38.03 & 3.83 \\

[\ion{O}{3}]$\lambda$5007 & $2884.32 \pm 21.47$ & 139.60 & 16.91\\

[\ion{O}{1}]$\lambda$6300 &  $566.94 \pm 4.20 $ & 21.80 & 3.05 \\

[\ion{O}{1}]$\lambda$6363 & $190.80 \pm 1.40$ & 7.26 & 1.02 \\
\Halpha & $2528.77 \pm 16.49$ & 109.46 & 13.65 \\

[\ion{N}{2}]$\lambda$6583 & $1951.50 \pm 10.41$ & 71.81 & 10.68 \\

[\ion{S}{2}]$\lambda$6716 & $976.91 \pm 5.33$ & 35.24 & 5.32\\

[\ion{S}{2}]$\lambda$6730 & $853.55 \pm 4.63$ & 30.72 & 4.61 \\ \hline\hline
\end{tabular}
\label{table:optlines}
\end{table}

For emission line measurements, we follow the procedure used in the OSSY database \citep{Oh11} and its broad-line prescription \citep{Oh15}. We perform stellar templates \citep{Bruzual03, Sanchez-blazquez06} and emission-line fitting in a rest-frame ranging from 3780~\AA\ to 7250~\AA\ (see bottom panel of Fig.~\ref{fig:sdss}). We correct the narrow line ratios ($H\alpha/H\beta$) assuming an intrinsic ratio of $R = 3.1$ and the \cite{Cardelli89} reddening curve. The measured Balmer decrement H$\beta$/H$\alpha=3.9$ suggests a low level of extinction of the narrow line region (NLR) and is consistent with the Balmer decrement for most optically selected AGN from the SDSS \citep[see Fig. 12 in][]{Koss17}. We measure the AGN emission-line diagnostics and confirm that NGC 5347 is consistent with a Seyfert galaxy using the [\ion{O}{3}]/\Hbeta\ vs.~[\ion{N}{2}]/\Halpha, \ion{S}{2}/\Halpha, and [\ion{O}{1}]/\Halpha\ diagnostics \citep[e.g.,][]{Veilleux87, Kewley06}. The observed characteristics of the major emission lines are reported in Table~\ref{table:optlines}.

The [\ion{O}{3}] line shows a blue wing consistent with an NLR outflow consitent with the outflows found in the HST data \citep{Schmitt03} and the extended emission observed with \textit{Chandra} (see next section for more details). We note that past observations had found no broad emission lines in the optical spectrum of the source \citep{degrijp92}. However, we found some evidence of residuals in the \Halpha-[\ion{N}{2}] complex that may be consistent with a weak broad line around \Halpha\ [$\rm EW(H\alpha_{\rm br})  = 10.38~ \AA$]. High-velocity wings associated with the outflow may be present in both the \Halpha\ and [\ion{N}{2}] line profiles and thus could be misinterpreted as an underlying broad \Halpha\ component associated with the broad line region (BLR). We note that most studies reported much more significant equivalent width of broad lines  \citep[e.g., $\rm \langle EW \rangle \sim 70\,\AA$;][]{Shen11}. \cite{Oh15} reported substantial number of unidentified weak broad-line in type 1 AGN in the local Universe ($z<0.2$) whose $\rm EW(H\alpha_{\rm br}) $ is peaking at $\sim 30~\AA$ \citep[see figure 9 in][]{Oh15}. To further understand the NLR outflows in this system and better detect or constrain possible weak broad lines, further observations would be required, such as high spatial resolution integral field NIR spectroscopy or spectropolarimetry.

\section{X-ray Observations and data reduction}
\label{sec:reduction}
NGC 5347 was observed by the \textit{Chandra X-ray Observatory} on 2004-06-05 (PI: N. Levenson; ObsID 4867), by \textit{Suzaku} on 2008-06-10 (ObsID 703011010), and by \textit{NuSTAR} (ObsID 60001163002) on 2015-01-16 . The log of the observations is presented in Table~\ref{table:log}. Here, we summarize our data reduction procedures.

\begin{table}
\centering

\caption{Net exposure time, average net count rate and the ratio of the source to total counts, in the observed 3--10\,keV band.}

\begin{tabular}{lccc}
\hline \hline
Instrument	&	Net exposure	&	Count rate	&	Source/total	\\
	&	(ks)	&	(count ks$^{-1}$)	&		\\ \hline
\textit{Chandra} (ACIS)	&	36.9	&	$4.44 \pm 0.36$	&	97.0~\%	\\
\textit{Suzaku} (XIS-FI)	&	42.0 	&	$3.17 \pm 0.44$	&	33.0~\%\\
\textit{NuSTAR} (FPMA)	&	46.5	&	$4.53 \pm 0.34$	&	84.8~\%	\\
\textit{NuSTAR} (FPMB)	&	46.6	&	$3.04 \pm 0.30$	&	76.1~\%	\\ \hline\hline

\end{tabular}
\label{table:log}
\end{table}
\subsection{\textit{ Suzaku} observations}

The XIS \citep{XIS} spectra from {\it Suzaku} \citep{Suzaku07} were reduced following standard procedures using {\tt HEASOFT}. The initial reduction was done with {\tt aepipeline}, using the CALDB calibration release v20160616. Source spectra were extracted using {\tt xselect} from circular regions 3$\arcmin$ in radius centered on the source. Background spectra were extracted from a source-free region of the same size, away from the calibration source. The response files were generated using {\tt xisresp}. We do not consider the spectrum from XIS1, owing to its poor relative calibration. Spectra from XIS0 and XIS3 were checked for consistency and then combined to form the front-illuminated spectra.

\subsection{\textit{ Chandra} observations}
\label{sec:chandra}

The \textit{Chandra} \citep{CXO00} data were reduced using CIAO version 4.9 and the latest associated calibration files. The source was observed close to the optical axis and nominal aimpoint on the backside-illuminated ACIS-S3 chip, meaning that the full spatial resolution of \textit{Chandra} can be exploited.

\begin{figure}
\centering
\includegraphics[width = 0.45\textwidth]{chandra_zoomin.eps}\\
\includegraphics[width = 0.45\textwidth]{Chandra_Spectra.pdf}
\caption{Top panel: \textit{Chandra} image of NGCC~5347 showing the 0.3-1.2~keV band (red), 1.2-2.4~keV band (green) and 2.4-8~keV band (blue). The image shows a clear spatial extension of the emission in the 0.3-1.2~keV band. \textit{Chandra} spectra extracted from the core of the source (blue points) and from the core and the extended emission (red points; see Sect.~\ref{sec:chandra}). We note that the O K emission (below $\sim 0.6$~keV) is stronger in the spectrum when the extended emission was included.}
\label{fig:Chandraspectra}
\end{figure}

Prior work noted that NGC 5347 is slightly extended in the \textit{Chandra} image. The diffuse emission region closely coincides with [\ion{O}{3}] emission detected in \textit{Hubble Space Telescope (HST)} images, potentially indicating the direction of an ionization cone or the NLR \citep[][]{Schmitt03, Levenson06}. Using sub-pixel event reprocessing and energy filtering, we are able to confirm that the extended X-ray emission is strongest in the soft band ($E \leq 1.5$~keV), and potentially strongest of all in the O K band (below $\sim 0.6$~keV), as shown in Fig.~\ref{fig:Chandraspectra}. The flux ratios of the spectrum including the extended region over the spectrum the core region are $1.35 \pm 0.10$ and $1.09 \pm 0.11$, below and above 1.5~keV, respectively.

Source and background spectral files and response files were all created using the CIAO tool {\tt specextract}. We first extracted source counts from a circular region with a radius of 1.5\arcsec\ (256~pc) centered on the known source coordinates, ignoring the extended emission. We then extracted the source and diffuse emission jointly using a 5.2\arcsec\ (891 pc) circle, centered on the extended image. The resultant data were grouped to require at least 10 counts per spectral bin.  The neutral Fe K line is clearly evident in the spectrum, and is several times stronger than the local continuum (see Fig.~\ref{fig:Chandraspectra}); this indicates that the central engine is highly obscured and signals that the source is CT. It is notable that the spectrum including the extended X-ray and [\ion{O}{3}] emission region has more flux in the O K range, consistent with neutral oxygen at 0.525~keV, or a low-ionization charge state. The flux of the Fe line in the spectrum, including the extended emission, is consistent with the one from the core, indicating that the Fe line is emitted within an inner region of 1.5\arcsec. For consistency, we use the spectrum that includes the extended emission in the rest of the analysis.

\subsection{{\it NuSTAR} observations}
The {\it NuSTAR} \citep{Harrison13} data were reduced following the standard pipeline in the {\it NuSTAR} Data Analysis Software ({\tt NUSTARDAS}\,v1.8.0), and using the latest calibration files. We cleaned the unfiltered event files with the standard depth correction. We reprocessed the data using the ${\tt saamode = optimized}$ and ${\tt tentacle = yes}$ criteria for a more conservative treatment of the high background levels in the proximity of the South Atlantic Anomaly. We extracted the source and background spectra from circular regions of radii 45\arcsec\ and 100\arcsec, respectively, for both focal plane modules (FPMA and FPMB) using the {\tt HEASOFT} task {\tt Nuproduct}, and requiring a minimum S/N of 3 per energy bin. The spectra extracted from both modules are consistent with each other. The data from FPMA and FPMB are analyzed jointly in this work, but they are not combined together.

\section{X-ray Spectral analysis}
\label{sec:spectral_fits}

Throughout this work, spectral fitting was performed using XSPEC\,v12.10e \citep{Arnaud96}. Due to the energy limitation of some of the employed spectral models in this work and the data quality, we considered the \textit{Chandra} and the \textit{Suzaku} spectra in the observed 0.6--8 keV and 0.7-- 7.5 keV bands, respectively. The \textit{NuSTAR} spectra are background dominated below 4~keV and above 30~keV. For that reason, we fit the \textit{NuSTAR} data in the  4--29~keV band. Given the consistency between the various instruments (Fig.~\ref{fig:spectra_model}a), we fixed the cross calibration between them to unity. Throughout this work, we apply the Cash statistic \citep[$C$-stat;][]{Cash79}. Unless stated otherwise, uncertainties on the parameters are listed at the 1$\sigma$ confidence level ($\Delta C= 1$). These uncertainties, for all the models, are calculated from a Markov chain Monte Carlo (MCMC) analysis, starting from the best-fitting model that we obtained. We used the Goodman-Weare algorithm \citep{Goodman10} with a chain of $10^6$ elements discarding the first 30\% of elements as part of the 'burn-in' period. We note that due to the non-Gaussianity in the distribution of some parameters, the best-fit value found using XSPEC does not match with the mean value found in the chains, however they are consistent within $2\sigma$.

First, we fit the spectra in the $1-5$ keV band, using an absorbed power-law model accounting for the Galactic absorption in the line of sight (LOS) of the source \citep[$ N_{\rm H, Gal} =  1.52 \times 10^{20}\, \rm cm^{-2}$;][]{Kalberla05}. The model fits the data well ($C/{\rm dof} = 19.3/20$) with a hard photon index $\Gamma = 0.81 \pm 0.14$. Such a hard spectrum indicates the presence of strong absorption. The extrapolation of the best-fit model to the $0.6-30$ keV band reveals the presence of an excess in the soft X-rays, a strong excess in the Fe-line band, and a broader excess in the $10-30$~keV band, as shown in Fig.~\ref{fig:spectra_model}b. The former component is mainly due to thermal diffuse emission, while the latter two components give strong indication that the hard X-rays in this source are dominated by reprocessed emission. In the following, we present a detailed analysis of the X-ray spectra (in the $0.6-30$~keV range) by considering different models in order to describe the reprocessed emission in this source.

\begin{figure*}
\centering

\includegraphics[width = 0.49\linewidth]{MYTD_data_model.pdf}
\includegraphics[width = 0.49\linewidth]{ratios.pdf}\\
\includegraphics[width = 0.6\linewidth]{NGC5347_corner.pdf}

\caption{ Upper panel: \textit{Suzaku} (black), \textit{Chandra} (red) and \textit{NuSTAR} FPMA/B (blue/magenta) spectra of NGC 5347. The grey line in panel (a) represents the best-fit MYTD model, in addition to the various components in the MYTD model. Panel (b) shows the ratio (data/model) by fitting the 1.5-5 keV band using a simple power law with $\Gamma = 0.85$. Panels (c), (d), and (e) show the residuals obtained by fitting Pexmon, MYTC and MYTD models, respectively. Lower panel: the confidence contours (showing the 1-$\sigma$, 2-$\sigma$ and 3-$\sigma$ levels) obtained from the MCMC analysis for the relevant parameters of the Pexmon (red) and MYTD (blue) models. The last panel in each row corresponds to the normalized 1-D probability density function of the corresponding parameter.}
\label{fig:spectra_model}
\end{figure*}

\subsection{Pexmon}
\label{sec:Pexmon}

We initially fit the spectra using the neutral reflection model Pexmon \citep{Nandra07}. The model can be written (in the XSPEC terminology) as follows:

\begin{eqnarray}
\begin{array}{lc}
{\tt model_{Pexmon} } & =  {\tt phabs[1] * ( zphabs[2]*cutoffpl[3]   }
\end{array}\nonumber\\
\begin{array}{lll}
  {\tt + zphabs[4]*constant[5]*cutoffpl[6]  } &
\end{array}\nonumber\\
\begin{array}{lc}
{\tt + pexmon[7] + mekal[8]}  ).&\nonumber
\end{array}
\label{eq:pexmon_model}
\end{eqnarray}

\noindent In this model, the {\tt phabs[1]} component represents the Galactic absorption, {\tt cutoffpl[3]} represents the primary emission of the source assumed to be a power-law with a high-energy cutoff (fixed to 500~keV), which is intrinsically absorbed by CT material ({\tt zphabs[2]}). A fraction (${\tt constant[5] *  cutoffpl[6]}$, where $0 \leq {\tt constant[5]} \leq 1$) of the primary emission could be scattered into our LOS, by optically thin ionized gas in the polar regions, before being possibly absorbed as well ({\tt zphabs[4]}). All the parameters of {\tt cutoffpl[6]} are tied to the ones of {\tt cutoffpl[3]}. The photon index, cutoff energy and normalization of {\tt pexmon[7]}, which describes the reprocess emission, are tied to the same parameters of {\tt cutoffpl[3]}. Finally, we describe the soft emission, which mainly arises from the extended regions, with a thermal diffuse emission, model {\tt mekal[8]}.

\begin{table*}
\begin{threeparttable}

\caption{Best-fit parameters obtained by fitting the spectra, using XSPEC, with Pexmon, MYTC, MYTD and Borus models. The values between brackets represent the mean value of each parameter and the corresponding 1$\sigma$ confidence interval obtained from the MCMC analysis. We also report the observed 2-10~keV fluxes and intrinsic luminosities for each model.}
\begin{tabular}{lllll}
\hline \hline
	Parameter			&	Pexmon	&	MYTC	&	MYTD	&	Borus	\\ \hline
$	N_{\rm H,\,LOS}\, (10^{24}\, \rm cm^{-2})		$	&	2.76 [3.43 (2.24, 4.45)]	&	--	&	4.67 [5.93 (3.86, 8.24)]	&	10 [5.81 (3.33, 8.51)]	\\
$	N_{\rm H,\,global} \, (10^{24}\, \rm cm^{-2})		$	&	--	&	10 [7.81 (6.17, 9.41)]	&	4.67$^t$	&	10$^t$	\\
$	\Gamma		$	&	2.4 [2.28 (2.18, 2.37)]	&	2.19 [2.20 (2.09, 2.31)]	&	2.33 [2.29 (2.22, 2.36)]	&	2.4 [2.11 (1.88, 2.33)]	\\
$	N_{\rm PL} \, (10^{-3})		$	&	2.46 [1.79 (1.33, 2.25)]	&	5.93 [9.81 (5.79, 13.99)]	&	6.61 [6.44 (5.15, 7.73)]	&	20.61 [5.49 (1.13, 9.91)]	\\
$	\theta_{\rm inc}		$	&	0$^f$	&	61.85 [68.77 (64.2, 73.3)]	&	--	&	63.38 [50.04 (34.7, 65)]	\\
$	\theta_{\rm torus}		$	&	--	&	--	&	--	&	60.65 [50.69 (38.2, 64.2)]	\\
$	\rm Abund		$	&	1.47 [1.40 (1.15, 1.62)]	&	--	&	--	&	1$^f$	\\
$	N_{\rm H,SC}\, (10^{22} \, \rm cm^{-2})		$	&	0.72 [0.88 (0.35, 1.36)]	&	0.25 [0.54 (0.19, 0.89)]	&	0.71 [0.76 (0.37, 1.13)]	&	0.72 [0.57 (0.27, 0.85)]	\\
$	f_{\rm SC} \, (10^{-3})		$	&	4.68 [9.22 (4.3, 13.3)]	&	1.39 [1.33 (0.64, 2.02)]	&	2.25 [2.58 (1.49, 3.67)]	&	0.93 [5.28 (1.44, 9.58)]	\\
$	kT_{\rm mekal}		$	&	0.68 [0.67 (0.62, 0.73)]	&	0.69 [0.67 (0.62, 0.74)]	&	0.67 [0.66 (0.61, 0.73)]	&	0.67$^f$	\\
$	N_{\rm mekal} \, ( 10^{-6})		$	&	4.56 [4.77 (3.86, 5.64)]	&	3.84 [4.45 (3.43, 5.43)]	&	4.70 [4.69 (3.78, 5.61)]	&	4.70$^f$	\\ \hline
$F_{2-10}\,(\rm 10^{-13}~erg~s^{-1}~cm^{-2})$ & $ 2.24^{+0.11}_{-0.07} $ & $2.34 \pm 0.11 $ & $2.32 ^{+0.10}_{-0.08}$ & $2.32 ^{+0.11}_{-0.07} $ \\
$L_{2-10}\,(\rm 10^{41}~erg~s^{-1})$ & $4.7 \pm 1.2$ & $15.2 \pm 7.6 $ & $14.4 \pm 2.9$ & $40.5 \pm 31.6$ \\ \hline
$	C/{\rm dof}		$	&	91.37/90	&	93.38/90	&	89.08/91	&	78.81/84	\\
\hline\hline
\end{tabular}
\begin{tablenotes}
	\item[$f$] fixed.
	\item[$t$] tied.
\end{tablenotes}
\end{threeparttable}
\label{table:param}
\end{table*}

The Pexmon model assumes an infinite slab responsible for the reprocessed emission. We were not able to constrain the inclination angle of the slab, so we fixed it to its best-fit value. We note that this angle represents the viewing angle of the reprocessing material itself and not of the whole system. We also fixed the reflection fraction to -1, so we account for the reflected emission only, assuming an isotropic primary emission. We left the Fe abundance (tied to the elemental abundance) free to vary.

This model fits the data well ($C/{\rm dof} = 91.37/90$). Throughout this work, we assess the goodness of the fits using simple Kolmogorov-Smirnov (KS) test in XSPEC, which estimates the largest difference ($\log D_{\rm KS}$) between the observed and model cumulative spectra. We also use the {\tt `goodness'} command in XSPEC by simulating 100 spectra based on the best-fit model and estimating the percentage of these simulations with the KS statistic less than that for the data (hereafter $p_{\rm KS}$). For this model, we found $\log D_{\rm KS} = -3.53$ and $p_{\rm KS} = 77\%$. The residuals are shown in Fig.~\ref{fig:spectra_model}c. The pexmon modelling implies that the emission in this source is absorbed by CT material with $N_{\rm H,\, LOS} = 2.76 \times 10^{24}\, \rm cm^{-2}$. Being heavily absorbed, the photon index of the primary emission could not be well constrained, so it was pegged to its maximum allowed value $\Gamma = 2.4$, with a lower limit of 1.95. The elemental abundance is found to be 1.45 times the solar abundance. We note that the scattered power-law emission is found to be $f_{\rm scat} = 0.47\%$ of the intrinsic primary emission, and absorbed by a material with $N_{\rm H, \, scat} =  7.2 \times 10^{21}\, \rm cm^{-2}$. The thermal mekal model adequately describes the soft X-rays with a temperature $kT = 0.68~ \rm keV$. The contour plots for the relevant parameters are shown in red in the lower panel of Fig.~\ref{fig:spectra_model}. Given the best-fit model, the intrinsic unabsorbed luminosity of the \textit{primary} emission is $L_{2-10} = (4.71 \pm 1.22)\times 10^{41}~~\rm erg\,s^{-1}$. The best-fit parameters for all models are listed in Table~\ref{table:param}.

\subsection{MYTorus}
\label{sec:MYT}

We next attempt to model the obscuration and the reprocessing emission by a CT torus using the MYTorus spectral-fitting suite for modeling X-ray spectra from a toroidal reprocessor \citep{MYT09}. We first consider the ``coupled'' configuration of MYTorus (hereafter MYTC). This configuration assumes that intrinsic emission is self-consistently absorbed and reprocessed by toroidal material with a circular cross section and half-opening angle of 60\degr\ and solar abundance. The viewing angle ($\theta_{\rm inc}$) and the global column density ($N_{\rm H,~global}$) of the torus are free parameters \citep[see][for more details about the various configurations of MYTorus]{Yaqoob12}. The model can be written as follows:

\begin{eqnarray}
\begin{array}{lll}
{\tt model_{MYTC} }  &=  {\tt phabs[1] *(  MYTZ[2] * zpowerlaw[3]  } &
\end{array}\nonumber\\
\begin{array}{lll}
  {\tt + zphabs[4]*constant[5]*zpowerlaw[6]  } &
\end{array}\nonumber\\
\begin{array}{lll}
{\tt+ constant[7]*MYTS[8] + constant[9]*MYTL[10] }
\end{array}\nonumber \\
\begin{array}{lll}
{\tt + mekal[11]} ). &\nonumber
\end{array}
\label{eq:MYTC}
\end{eqnarray}
\noindent
The ${\tt phabs[1]}$, ${\tt zphabs[4]*constant[5]*zpowerlaw[6]}$ and {\tt mekal[11]} components are equivalent to the ones in the Pexmon fit. {\tt MYTZ[2]} represents the attenuation of the intrinsic emission. {\tt MYTS[8]} and {\tt MYTL[10]} represent the scattered continuum and the fluorescent emission lines emitted by the torus. The {\tt constant[7,9]} factors correspond the relative weights of the three MYTorus components and are fixed to unity \citep[as suggested by][]{Yaqoob12}. We tried to link {\tt constant[7]} and  {\tt constant[9]} leaving the former free to vary. The quality of the fit was the same and we could not get any constraints on that parameter. We remind the reader that $N_{\rm H, LOS}$ can be estimated using $N_{\rm H,\, global}$ and $\theta_{\rm inc}$ by using eq. (1) in \cite{MYT09}. MYTorus does not have a high-energy cutoff. Imposing a cutoff energy to the primary emission would break the self-consistency of the models. Instead, MYTorus assumes various termination energies ($E_{\rm T}$). We used in our analysis the tables with $E_{\rm T} =500$~keV. Using different values did not affect the fits.

MYTC provides a statistically acceptable fit ($C/\rm dof = 93.38/90$, $\log D_{\rm KS} = -3.4$, $ p_{\rm KS} = 80\%$). The residuals are shown in Fig.~\ref{fig:spectra_model}d. This model also implies a CT absorber with $N_{\rm H, \, global} $ pegged to its maximum allowed limit of $10^{25} \, \rm cm^{-2}$ (the lower limit is $4.34\times 10^{24}\, \rm cm^{-2}$) and $\theta_{\rm inc}\sim 62\degr$. This suggests $N_{\rm H,LOS} \sim 3.4 \times 10^{24}\, \rm cm^{-2}$, consistent with the value obtained from the Pexmon fit. We found that $\theta_{\rm inc}$ is close to the half-opening angle of the torus. This implies that, in the context of a toroidal geometry, a considerable contribution to the reprocessed emission comes from the far side of the torus.

Next, we considered the decoupled configuration of MYTorus (hereafter MYTD) which is intended to mimic the Pexmon configuration. In this configuration, the viewing angle of {\tt MYTZ} is fixed to 90\degr, so its $N_{\rm H}$ corresponds to the LOS value. {\tt MYTS} and {\tt MYTL} are decomposed into two components, one from the near side of the torus ($\theta_{\rm inc}= 90\degr$) and the one from the far side of the torus ($\theta_{\rm inc} = 0 \degr$). The column densities of these component could be either tied to the one of {\tt MYTZ}, corresponding to a uniform distribution of the material, or free to vary (corresponding to a patchy structure). This model has only two more free parameters with respect to MYTC, which are the weights of {\tt MYTS} and {\tt MYTL}. MYTD can be written as follows:

\begin{eqnarray}
\begin{array}{lll}
{\tt model_{MYTD} }  &=  {\tt phabs[1] *(  MYTZ_{90}[2] * zpowerlaw[3]  } &
\end{array}\nonumber\\
\begin{array}{lll}
  {\tt + zphabs[4]*constant[5]*zpowerlaw[6]  } &
\end{array}\nonumber\\
\begin{array}{lll}
{\tt + constant[7]*(MYTS_0[8] + MYTL_0[9]) }
\end{array}\nonumber \\
\begin{array}{lll}
{\tt+ constant[10]*(MYTS_{90}[11] + MYTL_{90}[12]) }
\end{array}\nonumber \\
\begin{array}{lll}
{\tt + mekal[13]} ). &\nonumber
\end{array}
\label{eq:MYTD}
\end{eqnarray}
\noindent
For this configuration, we kept the column densities for all the {\tt MYT} components tied to the LOS value. Letting it be free resulted in a similar result. The relative weights for the {\tt MYTS} and {\tt MYTL} components with the same $\theta_{\rm inc}$ are tied together. First, we left {\tt constant[10]} free to vary. However, as expected from a CT absorption in the LOS, the reprocessed emission would be unlikely to escape the near side of the torus. Indeed, we find {\tt constant[11]} to be negligible ($< 10^{-5}$). Hence, we fixed it to zero in the rest of the analysis. We also fixed {\tt constant[7]} to unity which reduces the number of free parameters. We could not constrain it by leaving it free to vary. The model provides a statistically acceptable fit ($C/\rm dof = 89.08/91$, $\log D_{\rm KS} = -3.5$, $p_{\rm KS} = 79\%$). The best-fit parameters are listed in Table~\ref{table:param} and the residuals for this model are shown in Fig.~\ref{fig:spectra_model}e. The various components for this model are shown in panel (a) of the same figure. This figure shows clearly that the observed spectrum is dominated above $\sim 2$ keV by the reprocessed emission from CT material ($N_{\rm H,\, LOS} = 4.67 \times 10^{24}~\rm cm^{-2}$). The contour plots are shown in blue in the lower panel of Fig. \ref{fig:spectra_model}. All the parameters are consistent with the ones given by the Pexmon fit, except the normalization of the primary emission which is $\sim 2.7$ times larger than the value inferred by Pexmon. This is mainly due to the fact that the primary emission cannot be seen due to obscuration (see the red dotted line in Fig.~\ref{fig:spectra_model}a). Thus its intrinsic luminosity is estimated indirectly based on the reprocessed emission. This may lead to the discrepancy in the normalization of the primary due to different physical assumptions. Given the best-fit model, the observed 2-10~keV and 10-30~keV fluxes of this source are $(2.32 \pm 0.1)\times 10^{-13}\rm ~erg\,s^{-1}$ and $(1.16\pm 0.08)\times 10^{-12} \rm ~erg\,s^{-1}~cm^{-2}$, respectively. The intrinsic unabsorbed luminosity of the \textit{primary} emission is $L_{2-10} = (1.44 \pm 0.29)\times 10^{42}~\rm erg\,s^{-1}~cm^{-2}$. Thus, the intrinsic to observed flux ratio at $2-10$~keV is $103 \pm 23$.

\subsection{Borus}
\label{sec:borus}

Finally, we fit the spectra of the source by modeling the reprocessed emission using the Borus model \citep{Borus18}. Borus assumes a uniform density sphere with cutouts which are determined by the half-opening angle $\theta_{\rm torus}$ (a free parameter), giving a similar geometry to the one of MYTorus. The model can be described as follows:
\begin{eqnarray}
\begin{array}{lll}
{\tt model_{Borus} }  &=  {\tt phabs[1] *(  zphabs[2]*cabs[3] * cutoffpl[4]  } &
\end{array}\nonumber\\
\begin{array}{lll}
  {\tt + zphabs[5]*constant[6]*cutoffpl[7]  + Borus[8] } &
\end{array}\nonumber\\
\begin{array}{lll}
{\tt +  mekal[9]} ). &\nonumber
\end{array}
\label{eq:borus}
\end{eqnarray}
\noindent
The {\tt cabs[3]} component accounts for Compton scattering in the absorber, while the {\tt Borus[8]} accounts for the reprocessed emission. We note that the {\tt Borus} model is defined above 1~keV. For that reason, we fixed the parameters of the {\tt mekal[9]} component to the best-fit values obtained by the MYTD model and fitted the spectra above 1~keV. We tied $N_{\rm H,LOS}$ to the global value. We also tied the normalization of {\tt Borus[8]} to the one of {\tt cutoffpl[4]} whose high-energy cutoff is fixed to 500~keV. The abundance could not be constrained, so we fixed it to the solar value. The model gives a statistically acceptable fit ($C/\rm dof = 78.81/84$, $\log D_{\rm KS} = -3.5$, $p_{\rm KS} = 66\%$), also implying a CT source ($N_{\rm H,~ LOS} = 10^{25}\rm cm^{-2}$). We note that all the parameters are consistent with the values obtained by MYTD. Notably, $\theta_{\rm torus} \sim 60.4\degr$ is consistent with the one assumed by construction in the MYTorus model, which is 60\degr. The intrinsic unabsorbed luminosity of the \textit{primary} emission is $L_{2-10} = (4.05 \pm 3.16)\times 10^{42}~\rm erg\,s^{-1}$, consistent with the value obtained from the MYTD model.

\section{Discussion and conclusions}
\label{sec:discussion}

\begin{figure*}
\centering
\includegraphics[width = 0.49\linewidth]{Xrism_MYTD.pdf}
\includegraphics[width = 0.49\linewidth]{Athena_MYTD.pdf}
\caption{Simulated \textit{XRISM} (left panel) and \textit{Athena}/X-IFU (right panel) spectra of NGC 5347 assuming the best-fit MYTD model (red line) and an exposure time of 100 ks(in the observed frame). The inset in the right panel shows a zoom in on the 6--6.5~keV range, where the Fe K$\alpha$1,2 lines can be clearly resolved and separated together with the Compton shoulder. The vertical dotted lines show the fiducial energies of the Fe K$\alpha$1,2 lines assumed to be at 6.404~keV and 6.391~keV (rest frame), respectively. The spectra were grouped to require at least 10 and 25 counts per bin, for \textit{XRISM} and \textit{Athena}, respectively.}
\label{fig:Xrism-athena}
\end{figure*}

We have confirmed in this work the CT classification of NGC 5347. The $2-30$~keV multi-epoch spectra of this source are clearly dominated by reprocessed emission from CT material ($N_{\rm H} > 2.23 \times 10^{24}~\rm cm^{-2}$) obscuring the central engine. We note that this estimate is higher than the previously reported ones for this source \citep{Risaliti99,Lamassa11}. It is then possible that some sources which were classified as Compton thin could be in reality CT when higher-quality data covering a broader energy range and more physical models are used. \cite{Marchesi18} estimated $N_{\rm H}$ for 30 local AGN ($\langle z \rangle \sim 0.03$) from the \textit{Swift}/BAT 100-month survey that were observed by \textit{NuSTAR}. Our estimate puts the source in the upper quartile of the $N_{\rm H}$-distribution presented in Fig. 3 of \cite{Marchesi18}.

It is worth mentioning that all the models employed in this work are statistically comparable, giving statistically good fits and consistent physical parameters. However, the use of physically-motivated models such as MYTorus and Borus, accounting properly for the reprocessed emission in the torus, is preferred with respect to simple reflection models. We note that due to the faintness of the source, we were not able to get strong constraints either on the geometry of the obscuring material or on the properties of the intrinsic X-ray source. Our results are in alignment with the studies of megamaser AGN \citep[e.g.,][]{Greenhill08, Masini16} which revealed that a large fraction of megamaser AGN harbor a CTAGN.

Using the unabsorbed $L_{2-10}$ nuclear emission from the best-fit MYTD model, we solved the third-degree equation provided by \cite{Marconi04} (in their equation 21) to estimate the bolometric luminosity ($L_{\rm bol}$). We obtain $L_{\rm bol} = (1.65 \pm 0.33) \times 10^{43}~{\rm erg\,s^{-1}} \simeq 0.014 \pm 0.005~L_{\rm Edd}$. Moreover, by applying the $L_{2-10}-L_{\rm [O~III]}$ relationship for Seyferts found by \cite{Berney15}, we obtain $\log \left( L_{\rm [O~III]}/\rm erg~s^{-1} \right) \sim 40.14$ which is consistent with the values we obtained from the SDSS spectrum (see Fig.~\ref{fig:sdss}; $\log \left(L_{\rm [O~III]}^{\rm int.}/\rm erg~s^{-1} \right) = 40.11 \pm 0.03$) and the one estimated by \cite{Schmitt03} from \textit{HST} observations of this source. NGC 5347 is therefore consistent with the other sources analyzed by \cite{Ueda15} in both the $\log N_{\rm H} - \log \left[ L_{\rm [O~III]}/L_{2-10} \right] $ and the $\log \left[ L_{2-10}/L_{\rm Edd}\right] - \log \left[ L_{\rm [O~III]}/L_{2-10}\right]$ planes. However, the observed [\ion{O}{4}] luminosity \citep[$L_{\rm [O~IV]} = 1.15 \times 10^{40}~\rm erg~s^{-1}$;][]{wu11} is smaller than the inferred value ($L_{\rm [O~IV]} = 7.24 \times 10^{40}~\rm erg~s^{-1}$) obtained from $L_{\rm [O~IV]}-L_{2-10}$ correlation by \citep{Melendez08}. The two values are broadly consistent given the large uncertainties in this correlation. We note that the measured [\ion{O}{3}] and [\ion{O}{4}] fluxes could be underestimated if the NLR extends beyond the slit size of the instruments due to the closeness of the source. Finally, following \cite{Risaliti11} and \cite{Bis16}, if we assume that the [\ion{O}{3}] luminosity is an indicator of the intrinsic luminosity and is emitted isotropically, and that the underlying continuum is due to an optically thick accretion disk, then the observed [\ion{O}{3}] EW (EW$_{\rm obs}$) can give us an estimate of the orientation of the accretion disk. For an accretion disk that is observed with an inclination $\theta$, we get ${\rm EW_{\rm obs} = EW^\ast}/\cos \theta$, where ${\rm EW^\ast}$ is the EW as measured in a face-on configuration. Ideally the latter value is the same for all AGN. By considering an average value of $\rm EW^\ast$ to be $\sim 11~\AA$ \citep[see][who estimated $\langle \rm EW^\ast \rangle$ for a sample of SDSS quasars]{Risaliti11, Bis16}, and $\rm EW_{obs} = 16.91~\AA$ (see Table~\ref{table:optlines}), we obtain $\theta \sim 50\degr$.

Given the quality of the current data, we modeled the soft X-ray spectra ($E \leq 2~\rm keV$) using a fiducial model which assumes thermal diffuse emission. This model ensured a fair representation of the observed spectra at these energies. However, some of the emission could be due to photoionized plasma in the NLR. Understanding the nature of the soft X-ray emission in this source requires higher-quality data, which makes it an interesting candidate for future planned X-ray observatories carrying micro-calorimeters, such as \textit{XRISM} and \textit{Athena} \citep{Athena13}.

Future X-ray missions will allow us to obtain higher quality spectra by resolving all the line features in the spectra, enabling a better understanding of such sources. Fig.~\ref{fig:Xrism-athena} shows 100-ks simulated spectra using the response files of \textit{XRISM} (left panel) and \textit{Athena} /X-IFU\footnote{\url{http://x-ifu.irap.omp.eu/resources-for-users-and-x-ifu-consortium-members/}} \citep[right panel;][]{xifu13}, assuming the best-fit MYTD model. The faintness of the source would not allow the emission lines to be well resolved using XRISM. However, thanks to the large effective area of \textit{Athena}  all emission lines would be easily resolved. More interestingly, the inset in the right panel of this figure shows clearly that both Fe K$\alpha$1,2 lines (at rest-frame energies of 6.404~keV and 6.391~keV, respectively) would be separated and resolved, in addition to the corresponding Compton shoulder. This will enable a better identification and characterization of faint CT sources, with high-quality spectra. It will also allow us to study and identify the various spectral components in these sources, the geometry and covering fraction of the obscuring material. Any motion of the absorbing/reprocessing material whether it is orbital and/or outflowing will be then imprinted in the lines profile in terms of broadening and/or energy shift, and will be easily identified. Moreover, the rich emission line spectrum in the soft X-rays will allow us to study the various components contributing to this energy range such as the thermal emission from the host galaxy, or the extended emission from the NLR.

\begin{acknowledgements}
KO is an International Research Fellow of the Japan Society for the Promotion of Science (JSPS) (ID: P17321). We would like to thank Karl Forster for scheduling all of  the \textit{NuSTAR} observations in our program. We would like to thank Xavier Barcons, Fiona Harrison, Tim Kallman, Kirpal Nandra and John Raymond for useful conversations. This work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration.The results presented in this paper are also based on data obtained with the {\it Suzaku} observatory; and the {\it Chandra} X-ray Observatory. The figures were generated using matplotlib \citep{Hunter07}, a {\tt PYTHON} library for publication of quality graphics. The MCMC results were presented using the GetDist {\tt PYTHON} package.
\end{acknowledgements}

\software{pPXF \citep{Cappellari04}, CIAO \citep[v9.4][]{Ciao}, HEASoft \citep{HEASoft}, NUSTARDAS (v1.8.0, \url{https://heasarc.gsfc.nasa.gov/docs/nustar/analysis/}, XSPEC \citep{Arnaud96}, Matplotlib \citep{Hunter07}, GetDist (\url{https://getdist.readthedocs.io/en/latest/})}

\facilities{\textit{Chanrda X-ray Observatory}, SDSS, {\it NuSTAR, Suzaku.}}

redpajama_set_name: RedPajamaArXiv


text:
This Day in Liberal Judicial Activism—July 20
By Ed Whelan
About Ed Whelan
Follow Ed Whelan on Twitter
1990—After nearly 34 years of liberal judicial activism on the Supreme Court, Justice William J. Brennan, Jr. announces his retirement. As Jan Crawford Greenburg describes it in Supreme Conflict, "For conservatives, Brennan's retirement gave George H.W. Bush the chance of a lifetime.… It was that rare moment when a conservative president was positioned to replace a liberal giant.… It would give conservatives a dramatic opportunity to cement their majority and firmly take ideological control of the Court." But "the president did not want the kind of bruising fight over the Supreme Court that Reagan was willing to endure." Five days later President Bush nominates … David H. Souter to fill Brennan's seat.
Ed Whelan is the president of the Ethics and Public Policy Center and a regular contributor to NRO's Bench Memos. He is co-editor of The Essential Scalia: On the Constitution, the Courts, and the Rule of Law. @EdWhelanEPPC


text:
FOXBOROUGH, MA - JANUARY 15: A police officer receives his COVID-19 vaccination at Gillette Staium's vaccination site on January 15, 2021 in Foxborough, Massachusetts. First responders and healthcare workers will be first to recieve the vaccinations at the stadium, starting with around 300 people per day, but advancing to thousands per day soon after. (Photo by Scott Eisen/Getty Images)
Michelle Fiscus, Top Tennessee Health Official, Fired For Promoting COVID-19 Vaccines To Teens
by Gabrielle GuzJuly 17, 2021, 6:02 pmJuly 17, 2021, 6:02 pmJuly 17, 2021, 6:02 pmDaily Digest, News, News Feed >
Dr. Michelle Fiscus, a top health official in Tennessee, was fired from her job on Monday after she suggested that teens, ages 13-17, receive the COVID-19 vaccination. She worked as the Medical Director of Tennessee's Vaccine-Preventable Diseases and Immunization Program for the Department of Health.
While Fiscus was still in charge, the state's Department of Health was asked to appear before the Government Operations Committee because there was concern that Fiscus was putting pressure on children through Facebook messenger and other forms of advertisements to get inoculated without parental consent.
Fiscus has expressed concern about where her state is headed. In a 1,200-word response published in The Tennessean, she wrote that she is "angry for the amazing people of the Tennessee Department of Health who have been mistreated by an uneducated public and leaders who have only their own interests in mind."
Tennessee's former top vaccinations official, Dr. Michelle Fiscus, says the state's elected leaders put politics over the health of children by firing her for her efforts to get more Tennesseans vaccinated. Only 38% of Tennesseans are fully vaccinated. https://t.co/STyWcLQcks
She said that she is equally aggravated by the fact that the Tennessee Department of Health has stopped all outreach efforts for any vaccines for children.
The latest statistics show that only 38% of Tennesseans are fully vaccinated against COVID-19, which means that the state is lagging behind the rest of the nation.
Gov. Bill Lee (R) has declined to comment so far.
In a June committee meeting, some Republican lawmakers were angry because Fiscus sent a letter to medical providers who administered the vaccines and informed them about the state's legal mechanism that allows teenagers as young as 14 to get inoculated without parental consent. She said that the Health Department's Attorney provided the letter.
The agency terminated her on Monday, but no one told her of the precise reason why she was fired.
COVID-19 vaccine Dr. Michelle Fiscus Tennessee
Clarence Thomas Cites False Claims That Covid-19 Vaccine Stems From Aborted Cells In Decision
Alex Jones Calls Trump 'Ignorant' & 'Evil' For Supporting Vaccines
CDC Shortens Isolation Period For Covid-Positive People To 5 Days From 10
Article by Gabrielle Guz


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