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2014 Box Office: Bumpy Summer, Bumpy Year
By Jon The Blogcentric on 30 September 2014 | 1 Comment
You may have seen my blog about the VIFF already. One thing some people may not have noticed about my blogging is that I haven't been doing tracking of the year's box office pace. Normally I do. Maybe one or two of you have noticed. Anyways this is my first look at 2014 at the box office and it doesn't look too pleasant right now.
Decent Winter
The first quarter of 2014 didn't make as much as the first quarter of 2013. Nevertheless it did provide for an excellent January and February. Neither January or February set a box office record for that month but both outgrossed their respective month from 2013. January 2014 was almost $60 million higher than January 2013 thanks to hits like Frozen, Lone Survivor, Ride Along, The Wolf of Wall Street and The Nut Job. February 2014 was almost $175 million higher than February 2013 thanks to the phenomenal success of The LEGO Movie and other hits like The Monuments Men, About Last Night, Three Days To Kill, Non-Stop and Son Of God. However all that extra wouldn't be enough to outgross the winter of 2013 thanks to March 2014 grossing almost a quarter-billion less than March 2013. Strong openings for the 300 sequel, Mr. Peabody and Sherman, Divergent and Noah didn't carry far enough in the end and the winter of 2014 just missed by that much.
Spring Falls Slightly Short
Don't get me wrong. Spring was loaded with movies to get people to the cinema but it didn't outgross last year's spring. Once again no month set an all-time high but April was more than a quarter-billion higher than April 2013 thanks to Captain America 2, Rio 2, Heaven Is For Real and The Other Woman. May 2014 was more than $225 million shy of May 2013. Some could say there was no real big bang like Iron Man 3 from last year. Others could say too many competitors like The Amazing Spider-Man 2, Neighbors, Godzilla and X-Men: Days of Future Past opening at once.
However don't get me started on June. June was the month that sent the message that 2014 was going to have a tough summer at the box office. First off June had the only weekend where a movie released in 2014 grossed more than $100 million on its opening weekend: Transformers: Age of Extinction with a paltry $100,038,390. That's only 27th on the all-time list. Secondly were the ho-hum openings of movies like Maleficient, The Fault In Our Stars, 22 Jump Street, How To Train Your Dragon 2, and Think Like A Man Too. At the end of it all, June only grossed $995.4 million: $230 million less than June 2013 and the first June since 2003 to gross below $1 billion!
Summer's Bumpy Road
You shouldn't rely completely on the totals over at Box Office Mojo because the list of July totals shows July 2014 telling one story and the Weekly chart of 2014 and doing quick math in adding the July weeks telling another. One thing is certain is that this July didn't outgross July 2013 despite continuing success of Transformers 4 and openings for Dawn Of The Planet Of The Apes and Lucy.
The bright light not just of the summer but of the movie year so far has to be August. This is the one month that set an all-time record this year: $983 million. Definitely the success of the Guardians Of The Galaxy has a lot to do with it. There were other box office pumpers that month too like the Ninja Turtles, Into The Storm and Let's Be Cops.
I decided to pass up reviewing September even though it hasn't grossed as much as last year. Nevertheless the next three months will be a challenge. I don't think 2014 will set an all-time box-office record but it will draw huge crowds with Fury, Nightcrawler, Horns, the latest Hunger Games movie Mockingjay Part. 1 and sequels for Night At The Museum and Madagascar. I'm confident 2014 will end past $10 billion but that's something only time will tell.
"Yearly Box Office Chart" BoxOfficeMojo.com. 2013. Box Office Mojo. Owned by IMDB.com. http://www.boxofficemojo.com/yearly/
"Monthly Box Office Chart" BoxOfficeMojo.com. 2013. Box Office Mojo. Owned by IMDB.com. http://www.boxofficemojo.com/monthly/
"Weekend Box Office Chart" BoxOfficeMojo.com. 2013. Box Office Mojo. Owned by IMDB.com. http://www.boxofficemojo.com/weekend/
Posted in: Entertainment - Film and Movies, Showbiz	| Tagged: 2014, box office, flops, Galaxy, gross, Guardians, Hollywood, successes, summer, Transformers
It's VIFF Time Again
By Jon The Blogcentric on 24 September 2014 | Leave a comment
Yes, it's that time of year again. The Vancouver International Film Festival will be back up and running. It will open Thursday September 25th and run until Friday October 10th.
This year's festival looks to be optimistic. As you may remember, last year's festival could be considered a test pilot for the new way of doing the VIFF. They had no choice. The Granville 7–our main venue for years–closed in 2012 and a whole new system had to be created. It took finding new venues like the Vancouver Playhouse, the SFU Arts Centre, three cinemas of the International Village and the Rio Theatre and relocate their gala shows from the Vogue Theatre to the Centre for the Performing Arts. The end result was a success as it had one of the best per-screening averages. Sure there was a slight decrease in the number of films shown and the number of screenings but it payed off and kept the VIFF in a very healthy state.
There are not too many changes as far as screenings of films. One cool thing is that there will again be 11:30 showings at the Rio Theatre during certain nights. The festival promises to show 365 films from 70 countries during its duration. Some of the hot ticket films include:
Mommy– The latest film from 25 year-old Quebec directing phenom Xavier Dolan
Wild- A film starring Reese Witherspoon from Dallas Buyers Club director Jean-Marc Vallee
Maps To The Stars – A film by David Cronenberg with an excellent performance from Julianne Moore
Whiplash– a musical drama featuring drumming phenom Miles Teller
Welcome To Me– A dramedy starring Kristen Wiig that's surprisingly very personal
Clouds of Sils Maria– A humorous but personal story starring Juliette Binoche and Kristen Stewart
Foxcatcher– An Olympic story directed by Bennett Miller that ends up being far from the Olympic dream
Men, Women and Children– The latest Jason Reitman film that shows relationships of teenagers and their parents' relationships and the complications coming with it
The Riot Club– An intriguing look at special clubs and establishments in England in the 1800's
Winter Sleep– Cannes' Palme d'Or winner this year from Turkish director Nuri Bilge Ceylan
Goodbye To Language 3D– The latest from Jean-Luc Godard that caught the attention of crowds at Cannes.
The biggest change would be in the case of volunteering. In the past, volunteers would be kept strictly to a single theatre throughout the running of the festival. This time they can volunteer at any theatre or theatres they want. I myself have chosen to volunteer at three theatres so far. Yesterday at the volunteer orientation, all volunteers had to learn the five different duties which they will be assigned. This was the first time ever that the VIFF has given us instruction during the volunteer orientation. Nevertheless it's a good thing for when they have to do their duty.
Anyways the festival begins tomorrow. Expect a lot of excitement. And expect to see a good number of reviews from me. For more information or to purchase your own tickets, go to the VIFF website.
Posted in: Entertainment - Film and Movies, Showbiz, VIFF - Festival and Reviews	| Tagged: 2014, Cinematheque, Cineplex, Festival, film, International, Playhouse, Rio, Telefilm, Vancity, Vancouver, VIFF, Village
Move Review: Lucy
At first I was not interested in seeing Lucy. What got me seeing it was all the talk so many people who've seen it have said about it. I thought I'd check it out myself.
For those who haven't seen the movie, it's about a young woman who goes by the name of Lucy caught in a crime heist by surprise thanks to her shady and no-longer-living boyfriend. She then becomes a drug mule for a set of mind drugs that expands the brain's use at one time from the alleged normal 10% to as much as 100%. This sets her up with getting even with her crime bosses, connecting with the other drug mules involved and making sense with the human race thanks to a college professor and her own mind's supernatural ability to travel through time. Sound confusing? Well, you be the judge after you see the movie.
The funny thing about the movie is the whole plot of trying to make a connection between brain use at one time to the evolution of humanity coinciding with a criminal act. It's a movie that tries to be humorous as in the case of Lucy telling her roommate of her health condition as well as action-filled in the story of as well as try and provoke thought about the human race and people's ability to think. This is a complicated mix to try and create a good script that can entertain moviegoers.
One thing about the film is that it doesn't make complete sense. Yes it's a complicated story and yes there are parts that try to make it make sense over time. In fact the movie looked very ambitious at the beginning and appeared like it would deliver something to think about as the plot unraveled. However there are many times in which I wonder if it could have been organized out better or even played out better. Like those parts where Lucy connects with the ape-like human from eons ago made me question its purpose and whether it really worked or not. This is one case when I leave the movie theatre thinking of what scenes could have been done better and how. I will give credit to the effort by director/writer Luc Besson given to make such a movie that includes an intriguing story. In fact I found the best thing about the movie is the fact we never know Lucy's real name. But all the elements included in this story don't blend together well as a whole. I felt it to be uneven and confusing at times.
The movie did have a lot of positive qualities. The best thing about it had to be the acting. I can't complain about that. Scarlet Johansson and Morgan Freeman were good in their roles. They knew how to work their roles well otherwise the movie would have come across as completely ridiculous. They also knew how to keep our intrigue to the unfolding events. Choi Min-Sik and Amr Waked also acted well enough to keep the story intriguing and intact. The movies' special effects were also excellent, and for not even $40 million. The score to the film by Eric Serra also fit the story well.
One thing I have to say about Lucy is that it was actually successful in getting people to talk about the movie's topics. From the 10% brain-use hypothesis to the belief of evolution, that got a lot of people thinking, despite how disjointed the movie seemed. In fact I myself went to see it after two people I knew mentioned they saw it and gave their comments of what they thought of it. I find it interesting. That's all I will say. It also paid off at the box office too. It's still in theatres but it has made almost $125 million in North America and $378 million worldwide. I think the topic of the plot paid off in getting people to come. One feat it has achieved is this is Besson's highest-grossing film to date.
Lucy is an ambitious science fiction movie that tries to make us think while keeping us fixated on the story and the action along the way. However it's not all that together of a movie. Attention-grabbing, thought-provoking, but not really together.
Posted in: Entertainment - Film and Movies, Movie Reviews: 2014	| Tagged: 10, Amr, Besson, brain, Choi, Freeman, Johansson, Luc, Lucy, Min-Sik, Morgan, Scarlet, Waked
Movie Review: Guardians Of The Galaxy
By Jon The Blogcentric on 22 September 2014 | 3 Comments
Meet the Guardians Of The Galaxy: a superhero quintet that became household names this summer.
Oh boy. Now my time to catch up on movie reviews. This is the first of two reviews of summer blockbusters I saw. I will admit I've been a bit laxed in watching big movies this year. One of which I did feel I had to see was Guardians of The Galaxy. I'm glad I did.
I won't go into giving a brief description of the story since it's safe to assume most people have already seen it. This is one of those superhero movies that tries to balance out the comedic parts with the dramatic parts and the action parts. It does a very good job of it. It succeeds in giving the movie intriguing characters like Peter Quill, Gamora, Drax the Destroyer, Rocket and Groot. However like every first movie or introduction movie of a superhero or superhero ensemble, it has to have a very good story of how the superheroes came to be or in this case, came to be an ensemble. It does a good job of creating an introduction movie of such. It may not be as heavily dramatic as your typical superhero movie. It's a mix of drama and comedy that many will find entertaining. I will admit there are a couple of cornball scenes in there but the movie does a mostly good job.
I will admit that when I first saw the trailer for this months ago, I thought this would be a cheesy movie. I think what got me thinking it would be cheesy was seeing a raccoon as part of this superhero ensemble. It wasn't until I learned the Guardians Of The Galaxy movie is based off of a Marvel Comics series that I thought that this might be something good. I will admit I'm like a lot of people that probably never knew of the Guardians Of The Galaxy until I saw this movie. Anyone else? Yeah, I'm sure there are a bunch of you guilty of it too. Guardians Of The Galaxy has probably been one of Marvel Comics' least known comic heroes or hero ensembles. Actually the Guardians we know of are not the original Guardians. The first Guardians came out in 1969 and consisted of a different set of Guardians including one named Captain Marvel. Then came the 2008 ensemble of Guardians that consisted of some of the original characters but added in others like Groot, Rocket, Star Lord and Gamora but the total number of Guardians is in the dozens.
This also makes for an additional point for the challenge it had. Marvel and the producers had to work with creating a hit movie about a superhero ensemble that most of the general public are not very familiar with. It's definitely more challenging as doing such a movie with a more celebrated superhero like Superman or Captain America. The example of John Carter demonstrates the challenge; Disney hoped to introduce the world to John in a big way but it didn't work. Here it's Marvel's challenge to introduce the Guardians to the world and no doubt it would be a huge cost risk: $170 million to be exact. It paid off as it was the #1 movie for a total of five weekends. Its total box office is $313.7 million in North America and $632 million worldwide which is a modest number for a movie of that much success. Nevertheless I'll save it for when I give my upcoming movie year forecast. The movie's success also has paved the way for an upcoming sequel in 2017. The question is will they stick to the original five Guardians or will they add some additional Guardians in?
The first person who deserves acclaim for the success is director James Gunn. He hasn't had too huge of a resume as far as directors go. Actually he has a major blemish as he is one of the many directors with the atrocity Movie 43. However this is his breakthrough and should make a good name for him in the future. Possibly even a director of the sequel. Additional kudos to Nicole Perlman who co-wrote the script with Gunn. The collaboration paid off in giving a story full of action and humor and being what a script for a superhero movie should be.
Chris Pratt was entertaining as Peter Quill. He does a good job of balancing the role of a superhero with adding comedy plus he doesn't make dealing with his late mother too seriously dramatic. Zoe Saldana seems to be the actress made for sci-fi. First Avatar, then Star Trek and now this. Nevertheless I can't think of a better choice as she nails it again here. Dave Bautista also did a good job. And it's good to see since I don't normally think wrestlers make good movie stars as seen by past wrestlers. Bradley Cooper added great character to the voice of Rocket and Vin Diesel was good as Groot. Actually some of his better acting as of late. Other highlights include the visual effects of the movie which are probably some of the best of the year. Another plus is the inclusion of 70's music. At first you'd think it was cornball. However it becomes more evident why it's incorporated as it's this music that connects Peter to his mother. It also adds to the humor too.
Guardians Of The Galaxy is not just another good movie from the Marvel Comics team but a commercial achievement too in making household names of their lesser-known comic book characters. Good job.
Posted in: Entertainment - Film and Movies, Movie Reviews: 2014	| Tagged: Batista, Bradley, Chris, Comics, Cooper, Diesel, Drax, Galaxy, Gamora, Groot, Guardians, Gunn, James, Marvel, Peter, Pratt, Quill, Rocket, Saldana, Vin, Zoe
Movie Review: Boyhood
Boyhood is a movie of the growing years of Mason Evans Jr. (played by Ellar Coltrane) and was shot over a period of twelve years.
I know there have been a lot of people who liked my World Cup blogs but there are still some who feel like saying: "Jon, when's your next movie review?" For those wondering about that, yes I have been watching movies over the summer and I have a few reviews to share. To start with, I'll do Boyhood: a good choice for those who want something different.
The movie starts with six year-old Mason Evans Jr., a boy growing up in a small Texas town who's more interested in nature and collecting arrowheads than playing football. He lives with his slightly older sister Samantha, single mother Olivia and her boyfriend. Things are not the best as Mason has to share a bedroom with his sister and that causes typical brother-sister issues. Then it changes one day after an argument with Olivia and her boyfriend which she claims she has no free time. She moves to Houston with the children. This causes concern for mason wondering if he'll ever see his father again.
Life in Houston starts to work out fine for Mason and the family. Olivia is able to attend classes at the University of Houston while Mason and Samantha attend school. They're able to meet up with their father Mason Sr. but it's not so frequent. Even as Mason Sr. drops the kids off, friction between him and Olivia come back. In the meantime, Olivia meets up with Professor Bill Welbrock. He appears to be a good man with a head on his shoulders and even takes a liking to Mason, willing to introduce him to his own son Randy who's a similar like. The two marry and his children Mindy and Randy move in together. The family appears close knit as the stepsiblings have fun together and Bill appears to be the ideal husband. However things turn for the worse as Bill develops a drinking problem he first tries to keep secret only to have it exposed as he becomes abusive to Olivia and the children, even forcing Mason Jr. to get his head shaved. Olivia immediately leaves the household taking Mason and Sam with her.
The three find a new life in a town close to Austin. Olivia becomes a psychology teacher and falls in love with one of her students Jim who's a former Afghanistan War veteran whom she eventually marries. Mason Sr. has married and has become a father to a newborn. In the meantime, Samantha and Mason Jr begin social interaction of their own as they make friend and start dating. However Mason's drinking and earrings have gotten on the nerve of a visibly drunken Jim. Not surprisingly Olivia divorces him.
In the meantime Mason has a girlfriend named Sheena, works part-time at a seafood restaurant and has developed a passion for photography. His work in taking pictures and developing in the darkroom inspires him to be an artistic photographer. However it doesn't sit well with his teacher because he knows how competitive of a field photography is and how gimmicks are easier moneymakers than art. The teacher then makes Mason photographer for the football team.
Grade 12 is a life changing year for Mason Jr. Sam has moved onto college but she does allow Mason and Sheena to 'visit.' Sheena soon breaks up with Mason for a boy on the high school lacrosse team. Mason also wins second prize in a photography contest and receives scholarship money. His graduation is celebrated with family and others close in his life like his teacher and his boss at the restaurant. Going to college is the next chapter in Mason's life. However it's not without heartache as his mother finds it hard both her children have moved out and wonders of her own life. The film ends with Mason attending college, becoming friends with his roommate and being introduced to his roommate's girlfriend's best friend who shares a lot of common interests and common dreams with Mason.
Now this is something. Director Richard Linklater tells a story of Mason Jr. over the years and the people around him. He uses all the same actors, no replacements. This was very chancy because a lot can change over a period of twelve years. It's possible Ellar could have gotten tired of acting and wanted nothing to do with it anymore within that time. It's even possible one of the actors in one of the main roles could have died. Any one of them. But it worked. And it wasn't just simply the technical bits. It was also a story about a boy whose life over the years catches our intrigue. We're astonished to see Mason Jr. (or should I say Ellar?) grow over a twelve year span. We also see the lives of his mother, father and Sam pave their way too. All those who were part of the film and its 'aging process' contributed significantly. Also as it progresses over the time, Linklater doesn't leave anything out as far as aging goes. He doesn't get the adult actors to hide their facial aging. He doesn't replace the child actors if any one of them go through the 'awkward stage' or get braces. He keeps it all as is. That's another quality.
The thing is the film doesn't really tell the typical story that has a beginning, middle and end. Rather it tries to paint a portrait of Mason Jr. growing up over the years and of the boy he was and would grow up to be. It's not too thick on a plot but rather lets time unravel itself and tell the story as it goes along. Almost like childhood through Mason Jr's eyes. It's common with Richard Linklater's movies that they're not too heavy on the plot and give more of an atmosphere. Another thing this film can do is remind audience members of their own childhood growing up. It may tell a story of a boy who's not into sports and more of a dreamer but I'm sure there are some parts of Mason's childhood that will remind them of their own.
Another additional element that adds to the film are the surrounding scenes that add to the atmosphere. Linklater has done that in past films where he would show elements in the film that would actually add to it. We see it here too with Sam's like of popular culture from Britney Spears to High School Musical to Lady Gaga. We see it in the computer technology as the cast go from Apple computers with big box screens to iPhones. We see it in Mason Jr. growing up in highly conservative Texas and the values the state tries to instill with the people and through the schools. We also see it in how it with Mason Sr. being a liberal Democrat in a state that has a lot of staunch conservatives. We also see it with scenes with other artistically-minded people in the film. It all adds to it.
This film also adds to a common theme of Richard Linklater's movies. Linklater has never been one to dwell into the typical Hollywood fanfare. He's always been one to do his movies his way. His movies have featured people pursue their passion and even dream out loud. He often focuses on the visionaries and the inspired ones and he presents them as the ones to be admired. I think that's why he has such a following with Generation X. We can see that in Mason Jr. He falls in love with photography and wants it to be his life passion. The problem is those around him don't think highly of his choice. The teachers question it and whether it's a career choice that will allow for a decent living. His father wonders why he doesn't pursue something that 'wins chicks.' His girlfriend drops him for a jock because it doesn't make him look cool enough. And his friends razz him about it. But it's his passion. I think that's what Linklater is showing. About how passion is what matters. Especially for a boy like Mason.
Without a doubt, this is an accomplishment from Linklater. It was a unique idea from him that was creative but risky and it paid off very well. However this is also an accomplishment from actor Ellar Coltrane. It was not an easy job to play the same role over twelve years of filming. Nevertheless he did an excellent job in the role. It wasn't so much a role filled with emotional range or drama but rather a role that required the actor to grow along with the role and have the personality of the dreamer Linklater intended to have as the central protagonist. Much of it was natural personality but a lot of it was maturity over age. And Ellar did it. Very excellent.
Patricia Arquette was also very good as the mother almost to the point it appeared she stole the movie. The movie was also about the mother over the years improving her life, raising her two children and falling into two marriages that appeared right at the time but would soon make a turn for the worse. Her struggles added to the story not just to add to Mason Jr's story but to also mix it in as her own story too. Ethan Hawke was also good as the father who makes the annual visit. He too shows maturity over the years but his overall role was not as challenging as his past roles. Lorelei Linklater was also very good. She may have been cast as Sam simply because she's Richard Linklater's daughter–much the same way Ethan was cast because of working in his Before Sunrise series– but she wasn't just simply there. She was given a role too that involved her to grow along with Ellar and also portray Sam as this sister who was liked pop culture, had her own individual style, had ambitions of her own and was a typical older sister in both the fun times and the bad times with Mason.
One thing to note as well. It has been noticed in the last few years the lack of buzz alternative or independent cinema has had over the years. There hasn't as big of a phenomenon from Sundance or any other film festival promoting independent film in the last while. I don't know if Boyhood would qualify as a phenomenon but it is one film that has gotten bigger notice over time and has grown with the buzz. It currently has made $22 million in the US and $37 million worldwide. It has also received a lot of critical admiration and a lot of praise for its uniqueness. Definitely a big boost for independent cinema this year.
Boyhood is one of those summer movies one who wants to get off the beaten path of your typical summer movie fanfare would want to see. It's definitely worth it.
Posted in: Movie Reviews: 2014, Oscars 2014: Best Picture Reviews	| Tagged: Arquette, Boyhood, Coltrane, Ellar, Ellar Coltrane, Ethan, Hawke, Linklater, Lorelei, Mason Evans Jr., Patricia, Richard, Richard Linklater, Texas


MOUNTAIN VIEW, Calif. – Sept. 29 (SEND2PRESS NEWSWIRE) — Gen-9, Inc. (www.gen-9.net) announced today the Beta release of a new personal information management (PIM) software application called NOAH. NOAH integrates the management of email, Web pages, RSS feeds, contacts, scheduling, application files and other data into a single, customizable, easy to use client interface. The product will initially be available in a limited Beta release, to be followed by a general release by the end of the year.
A recent survey shows that after using organizers and PIMs for over 6 months, 50% of users abandoned them, and only 15% said that the software really helped them become more efficient. Noah takes a different approach to organizing and managing information that is both Internet centric and very intuitive. The developers expect that the innovative features in Noah will make it valuable to both the casual user and the power user.
Noah runs from the user's PC using a local database. Gen-9 will be making the single user version available as a free download. It plans to introduce an enterprise version in 2007. Free downloads will be made available at www.gen-9.net .
Original Keywords: NOAH, personal information manager, PIM, beta software release, Gen-9 Inc, Mark A. Fauci, management of email, Web pages, RSS feeds, contacts, scheduling, application file Gen-9, Inc.
REFERENCES: Software News, NOAH, personal information manager, PIM, beta software release, Gen-9 Inc, Mark A. Fauci, management of email, Web pages, RSS feeds, contacts, scheduling, application file Gen-9, Inc.


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Евгений Игоревич Тамм (16 ноября 1926 — 26 января 2008) — доктор физико-математических наук, лауреат Государственной премии СССР (1973), мастер спорта СССР (1962), заслуженный тренер СССР (1982) по альпинизму.

Заведующий сектором физики высоких энергий ФИАН им. П. Н. Лебедева, председатель Всесоюзной секции альпинизма ДСО «Буревестник», заместитель Председателя Президиума Федерации альпинизма СССР (1976—1977), Председатель Президиума Федерации альпинизма СССР (1978—1981). Руководитель и тренер сборов по подготовке Гималайских экспедиций (1978—1981). Начальник первой Советской Гималайской экспедиции (1982). Автор более 80 печатных научных работ и ряда альпинистских публикаций.

Биография
Евгений Игоревич Тамм родился 16 ноября 1926 года в Москве.

В 1940 году вместе с отцом, Игорем Евгеньевичем Таммом, совершил своё первое восхождение на вершину Сунахет.

В 1943 году поступил в Московский авиационный институт, позднее перевелся в Московский механический институт боеприпасов. После защиты диплома занимался экспериментальными работами в области физики высоких энергий.

В 1961 году команда альпинистов под руководством Тамма получила золотые медали в классе высотных восхождений Чемпионата СССР за восхождение на Пик Коммунизма.

В 1962 году получил звание «Мастер спорта СССР».

С 1957 по 1972 год руководил сборами и экспедициями на Кавказ, Памир, Тянь-Шань и Алтай.

В 1973 году удостоен Государственной премии СССР в составе научного коллектива за цикл работ «Фоторождение пи-мезонов на нуклонах».

С 1978 по 1981 годах являлся руководителем и тренером сборов по подготовке Гималайских экспедиций.

В 1982 году являлся Начальником первой советской гималайской экспедиции, покорившей вершину Эверест, за что ему было присвоено звание «Заслуженный тренер СССР».

В 1999 году удостоен Премии имени П. А. Черенкова за серию работ по созданию ускорительного комплекса ФИАН в городе Троицке и проведение экспериментов по физике высоких энергий.

В последние годы жизни страдал от болезни Паркинсона. Скончался 26 января 2008 года. Похоронен рядом с могилами родителей, в Москве, на Новодевичьем кладбище.

Ссылки
 Биография Е. И. Тамма на сайте «Космический мемориал»
 Биография Е. И. Тамма на сайте клуба альпинистов «Санкт-Петербург»
 Воспоминания Е. И. Тамма «60 лет с ФИАН» (2001)
 Интервью в газете «Советский спорт» (2007)

Альпинисты СССР
Лауреаты премии имени П. А. Черенкова
Чемпионы СССР по альпинизму
Сотрудники ФИАН
Физики СССР
Физики России
Доктора физико-математических наук
Похороненные на Новодевичьем кладбище

redpajama_set_name: RedPajamaWikipedia


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Q: How do I manually update my custom rom's security patches using 'git cherry-pick'? I made a custom rom for my device using Resurrection Remix Nougat. However, the security patch of the rom is December 5, 2017. I've found a guide that gives instructions (https://thealaskalinuxuser.wordpress.com/2016/08/29/how-to-manually-update-your-custom-rom-source-code-with-security-updates/) but it says to manually edit the files, even though there are commit codes on the pages (ex: https://android.googlesource.com/platform/frameworks/base/+/4afa0352d6c1046f9e9b67fbf0011bcd751fcbb5)
Is there a way to add these commits using 'git cherry-pick' or something else without manually editing the files?
I have tried the following (with this example: https://android.googlesource.com/platform/frameworks/base/+/4afa0352d6c1046f9e9b67fbf0011bcd751fcbb5)

*

*go to frameworks/base using 'cd frameworks/base'

*'git fetch https://android.googlesource.com/platform/frameworks/base'

*'git cherry-pick 4afa0352d6c1046f9e9b67fbf0011bcd751fcbb5
After running the chery-pick command, I get this:
fatal: bad object 4afa0352d6c1046f9e9b67fbf0011bcd751fcbb5

A: Try:
git fetch https://android.googlesource.com/platform/frameworks/base  4afa0352d6c1046f9e9b67fbf0011bcd751fcbb5 --depth 2
git cherry-pick 4afa0352d6c1046f9e9b67fbf0011bcd751fcbb5

And here's another method. Press the button diff on the page of https://android.googlesource.com/platform/frameworks/base/+/4afa0352d6c1046f9e9b67fbf0011bcd751fcbb5, and the diff/patch of the commit is displayed, which starts with the line
diff --git a/core/java/android/net/Uri.java b/core/java/android/net/Uri.java

You can copy and paste the diff into a local file, foo.diff for example, and run
git apply foo.diff

A: 'go to frameworks/base using 'cd frameworks/base'
'git fetch https://android.googlesource.com/platform/frameworks/base' -A
'git cherry-pick 4afa0352d6c1046f9e9b67fbf0011bcd751fcbb5

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ICHSA
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Water supply system management
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Optimization algorithms (Meta-heuristics)
International journal papers
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Conference papers and book chapters
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HSA website
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Conference papers and
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International journal papers download list
156 2022 H.S. Choi, J.H. Kim, E.I. Lee, S.K. Yoon, "Development of a Revised Multi-Layer Perceptron Model for Dam Inflow Prediction" Water, Vol.14, Issue.12, Dec (SCIE)
155 2021 J.H. Kim, "CACAIE: The Best Compendium for Nature-inspired Algorithms and their Applications in Civil Engineering" Computer-Aided Civil And Infrastructure Engineering, Vol.36, Issue.12, Dec 2021 (SCIE)
154 2021 S.H. Kwon, J.H. Kim, "Machine Learning and Urban Drainage Systems: State-of-the-Art Review " Water, Vol.13, Issue.24, Dec 2021 (SCIE)
153 2021 D.E. Chang, D.G. Yoo, J.H. Kim, "A Study on the Practical Pressure-Driven Hydraulic Analysis Method Considering Actual Water Supply Characteristics of Water Distribution Network " Sustainability, Vol.13, Issue.5, Mar 2021 (SCIE)
152 2021 S.H. Kwon, D. Jung, J.H. Kim, "Optimal Layout and Pipe Sizing of Urban Drainage Networks to Improve Robustness and Rapidity" Journal of Water Resources Planning and Management, ASCE, Vol.147, Issue.4, April 2021 (SCIE)
151 2020 S. Lee, J.H. Kim, "Quantitative Measure of Sustainability for Water Distribution Systems: A Comprehensive Review" sustainability, Vol.12, Issue.23, Dec 2020 (SCIE)
150 2020 Y.H. Choi, A. Sadollah, J.H. Kim, "Improvement of Cyber-Attack Detection Accuracy from Urban Water Systems Using Extreme Learning Machine" Applied Sciences, Vol.10, Issue.22, Nov 2020 (SCIE)
149 2020 D. Paez et al, "Battle of Postdisaster Response and Restoration" Journal of Water Resources Planning and Management, ASCE, Vol.146, Issue.8, Aug 2020 (SCIE)
148 2020 H.J. Kim, J.H. Kim, U. Ji, S.H. Jung "Effect of Probability Distribution-Based Physical Habitat Suitability Index on Environmental-Flow Estimation" KSCE Journal of Civil Engineering, Vol.24, Issue.6, pp.2393-2402, Jun 2020 (SCIE)
147 2020 F. Jafari, S.J. Mousavi, J.H. Kim, "Investigation of Rainfall Forecast System Characteristics in Real-Time Optimal Operation of Urban Drainage Systems" Water Resources Management, Vol.34, Issue.5, pp.1173-1787, Apr 2020 (SCIE)
146 2020 S.H. Kim, S. Eghdamirad, A. Sharma, J.H. Kim, "Quantification of Uncertainty in Projections of Extreme Daily Precipitation" Earth and Space Science, Vol.7, Issue.8, Aug 2020 (SCIE)
145 2020 D.E. Chang, D.G. Yoo, J.H. Kim, "Practical Head-Outflow Relationship Definition Methodology That Accounts for Varied Water-Supply Methods" Sustainability, Vol.12, Issue.11, Jun 2020 (SCIE)
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Alexandria Ocasio-Cortez won't take office until January, but the progressive firebrand is already casting herself as the voice of the people in the debate over Amazon's arrival in New York, even as fellow Democrats rushed to welcome the company.
"Amazon is a billion-dollar company," Ocasio-Cortez wrote on Twitter late Monday. "The idea that it will receive hundreds of millions of dollars in tax breaks at a time when our subway is crumbling and our communities need MORE investment, not less, is extremely concerning to residents here."
Amazon formally announced its choice Tuesday morning, naming New York and a location just outside of Washington, DC, to share its 50,000-employee second headquarters.
The announcement included welcoming comments from New York Mayor Bill de Blasio and New York Democratic Gov. Andrew Cuomo, who joked to reporters earlier this month that he would change his name to "Amazon Cuomo, if that's what it takes" to lure the tech behemoth.
"Today, with Amazon committing to expand its headquarters in Long Island City, New York can proudly say that we have attracted one of the largest, most competitive economic development investments in US history," Cuomo said in his statement.
New York State will grant $1.525 billion in incentives contingent on the company creating 25,000 new jobs with an average salary of $150,000 and occupying a certain amount of office space.
Ocasio-Cortez joined a skeptical chorus that already includes state senator Michael Gianaris and Queens City Council Member Jimmy van Bramer, who have voiced their opposition to any tax breaks for Amazon.
They may have more political power to push back against those incentives following last week's elections, in which New York Democrats took back the state senate.
From her perch as the surrounding area's representative in Congress, Ocasio-Cortez has little authority over the deal. But her tweets Monday and Tuesday on the deal showed her power as a progressive darling to rally local activists and officials to influence how the deal is implemented — including holding Amazon accountable.
In the rest of her tweet thread, Ocasio-Cortez outlined demands that commonly are featured in community benefits agreements negotiated between developers and local residents, such as well-paid jobs, protections for unions and investments in neighborhood infrastructure. Long Island City has undergone a blistering pace of high-end apartment construction in recent years, sending housing prices soaring.
"Displacement is not community development. Investing in luxury condos is not the same thing as investing in people and families," she wrote. "Shuffling working class people out of a community does not improve their quality of life."
In its announcement, Amazon said it would build space for a tech incubator and a new public school in Long Island City. Through a payment-in-lieu-of-taxes agreement, the company will invest in neighborhood infrastructure improvements and green spaces. It did not mention provisions for affordable housing.
A spokesperson for Ocasio-Cortez did not immediately return a request for comment. The congresswoman-elect on Tuesday morning was leading a sit-in with climate change protesters at the Capitol in Washington.


text:
\section{Introduction}

The intracluster medium (ICM) contains a large amount of metals, which
are synthesized by supernovae (SNe) Ia and SNe II in cluster galaxies.
A knowledge of the contributions from the two types of SNe to the metal abundances are important
to  understand
the origin of the metals and to study the evolution of galaxies in clusters.

The XMM-Newton observatory  enables us to derive O and Mg abundances, which
are not synthesized by SN Ia.
For the ICM of M 87 observed with the  XMM,
the O/Si ratio is found to be about a half of the solar ratio, while
Fe and Si have  similar values in units of the solar abundance
(B\"ohringer et al. 2001; Finoguenov et al. 2002; Matsushita et al. 2003).
Such low O abundances compared to the Si abundances are also
derived for the centers of other clusters and groups of galaxies
(e.g. Tamura et al. 2001b ; Boute et al. 2003, and others).

In order to  account for the observed O/Si/Fe abundance pattern of M 87,
the Fe/Si ratio of ejecta of SN Ia should be about 1
solar ratio. This value is significantly higher than expected
and probably  related with dimmer SNe Ia observed in old
stellar systems (Hamuy et al. 1996; Ivanov et al. 2000).
Since the mass of synthesized Ni$^{56}$ determines the
luminosity of each SN,
the abundance ratio in the ejecta may be correlated to  the luminosity
of SN Ia.
 In this context a lower Ni$^{56}$ yield implies less complete
nuclear burning with a higher ratio of $\alpha$-elements such as Si to Fe.
The observed O/Si/Fe pattern of the Galactic stars
 also indicates that the Si/Fe ratio in ejecta of SN Ia depends on stellar
metallicity, i.e., age of  the system (Matsushita et al. 2003)

The variation in the observed abundance pattern reflects variations in the
 explosion models, e.g. a high fraction of Fe for the classical deflagration model, W7
(Nomoto et al. 1984) or a larger fraction of Si for the delayed detonation model, WDDs
(Nomoto et al. 1997; Iwamoto et al. 1999).
The W7 model,  which can well reproduce observed optical spectra of SNe Ia
(Nugent et al. 1997), predicts a high Fe/Si ratio of 2.6 in units of the
solar ratio.
In contrast, the WDD models give a wider range of
Fe/Si ratios from 1 to 3 in units of the solar ratio, which might be related to the age of
the system (Umeda et al. 1999).

In this paper, we report on the O/Mg/Si/Fe abundance pattern of the Centaurus
cluster observed with XMM.
 The temperature properties of the cluster are described in Takahashi (2004).
The Centaurus cluster is a nearby cluster, centered on the cD galaxy,
 NGC 4696.
A positive temperature gradient and a negative abundance gradient are observed
with ASCA  (Fukazawa et al.1994; Ikebe et al.1999).
The cluster is expected to have a cooling flow  (Allen \& Fabian 1994),
and Chandra observed an  unusual plume-like cool structure at the center
(Sanders \& Fabian 2002).
 However,  as in other cooling flow clusters,
 the luminosity of the central cool component is much
smaller than the expected value from the cooling flow model (e.g. Makishima
et al. 2001; Tamura et al. 2001a; B\"ohringer et al. 2002; Matsushita et
al. 2002).
The problem of the missing of the cooling component becomes an advantage in
determination of elemental abundances, since the observed narrow temperature range of the ICM
 strongly reduces the ambiguity in the abundance measurement.

We adopt for the solar abundances the values given by Feldman
(1992), where the solar  Fe abundance relative to H is
3.24$\times10^{-5}$  in number.
 A value for the Hubble constant of $H_0=70 ~\rm{km/s/Mpc}$ is assumed.
Unless otherwise specified, we use 90\% confidence error regions.

\section{Observation}

The Centaurus cluster was observed with XMM-Newton on January 3rd, 2002.
 The thin filter is used for the EMOS and the EPN.
We have selected events with pattern smaller than 5 and 13 for the EPN and
the EMOS, respectively.
The background spectrum was calculated for each spectrum
by integrating blank sky data in the same detector regions.
Among deep sky observations collected with  XMM, we have selected the data
with the most similar background to that of the Centaurus cluster,
after screening  background flare events in the data and the background
following Katayama et al. (2004).
The effective exposures of the EPN and the EMOS are 29 ks and 32 ks, respectively.
The spectra  are  accumulated within rings, centered on the X-ray peak of the cluster.
After subtracting the background and correcting for the effect of  vignetting,
 deprojected spectra are calculated  assuming spherical symmetry.
For the EPN spectra, the response matrix  file  and the auxiliary response file  corresponding
to each spectrum are calculated using  SAS-v5.4.1.
For the EMOS data,  we used m1\_thin1v9q20t5r6\_all\_15.rsp.
The spectral analysis uses the XSPEC\_v11.2.0 package.
For the EPN data, we used the spectral range from 0.5 to 7.3 keV,
in order to discard strong instrumental lines around 8 keV.
We fitted  the  EMOS data in the spectral range from 0.4 to 9.0 keV.
 At $r>8'$, the energy range of 1.45--1.55 keV of the EMOS
is discarded
due to a  strong instrumental line.
Here, $r$ is the projected radius from the X-ray peak.
We also denote $R$ as the deprojected or three-dimensional radius.

\section{Spectral fit with the MEKAL model}

 The first step of the analysis is fitting the annular (projected) spectra
with a single temperature MEKAL  (e.g. Kaastra  1992; Liedahl et
al. 1995) model,
and the  deprojected spectra  with a single and two-temperature MEKAL
model with photoelectric absorption.
Abundances of C and N are fixed to be 1 solar and those of other
elements are determined separately.
The abundances of each element for all temperature
components are assumed to have the same values.
In addition, the deprojected spectra are fitted with a multi-temperature model which
is a sum of 14 temperature components.
 Since a spectrum from  an isothermal plasma can be well reproduced by a sum of
spectra of plasma of two neighboring temperatures  with similar elemental abundances,
we selected temperatures in order to derive  metal abundances with an
accuracy within 5 \%.
Thus, in order to determine the abundance distribution, this multi-temperature
model is enough to fit any
temperature distribution at least when all temperature components have
the same abundances.

\begin{figure}[]
\resizebox{8.1cm}{!}{\includegraphics{AA1577_figure1.ps}}
\caption{The deprojected spectrum at $R$=0.5--2$'$ of the EMOS1+EMOS2 of the Centaurus cluster fitted with
 the single temperature MEKAL model (black thin lines), the
 two-temperature MEKAL model (black dotted lines),
 the multi-temperature MEKAL model (black bold lines), and the
 multi-temperature APEC model (gray bold lines).
}
\label{depro_abund}
\end{figure}

\begin{table*}
\caption{Results of spectrum fitting of the projected spectra.}
 \begin{tabular}[t]{rlllllllllr}
 $r$     &  &   & kT &   & $N_{\rm H}$ & O & Mg & Si  & Fe &  $\chi^2/dof$\\
(arcmin)& && (keV) & (keV) & (10$^{20}{\rm cm^{-2}}$) & (solar)&
  (solar)& (solar)& (solar)& \\\hline
  0.05- 0.25 &EMOS &1T &1.00& &17.8& 0.00& 0.09& 0.28& 0.34& 837/ 61 \\
 0.25- 0.50 &EMOS &1T &1.36& &15.0& 0.25& 0.00& 0.47& 0.67& 740/ 96 \\
 0.50- 0.70 &EMOS &1T &1.66& &11.8& 0.33& 0.09& 1.01& 1.20& 386/ 93 \\
 0.70- 1.00 &EMOS &1T &1.89& &10.9& 0.44& 0.18& 1.31& 1.50& 483/127 \\
 1.00- 1.40 &EMOS &1T &2.42$^{+0.05}_{-0.05}$ &&9.4$^{+0.6}_{-0.6}$& 0.64$^{+0.19}_{-0.18}$& 0.28& 1.60$^{+0.17}_{-0.16}$& 2.04$^{+0.13}_{-0.12}$& 283/148 \\
 1.40- 2.00 &EMOS &1T &2.77$^{+0.05}_{-0.05}$ &&8.8$^{+0.5}_{-0.5}$& 0.50$^{+0.17}_{-0.16}$& 0.41& 1.58$^{+0.15}_{-0.14}$& 1.83$^{+0.09}_{-0.09}$& 266/169 \\
 2.00- 2.80 &EMOS &1T &3.00$^{+0.05}_{-0.05}$ &&8.8$^{+0.4}_{-0.5}$& 0.70$^{+0.17}_{-0.16}$& 0.56& 1.43$^{+0.14}_{-0.13}$& 1.66$^{+0.08}_{-0.08}$& 307/193 \\
 2.80- 4.00 &EMOS &1T &3.32$^{+0.06}_{-0.06}$ &&9.2$^{+0.4}_{-0.4}$& 0.60$^{+0.15}_{-0.15}$& 0.31& 0.98$^{+0.12}_{-0.12}$& 1.14$^{+0.06}_{-0.06}$& 331/224 \\
 4.00- 5.60 &EMOS &1T &3.60$^{+0.07}_{-0.07}$ &&8.2$^{+0.4}_{-0.3}$& 0.37$^{+0.14}_{-0.14}$& 0.48& 0.78$^{+0.11}_{-0.11}$& 0.80$^{+0.05}_{-0.05}$& 329/240 \\
 5.60- 8.00 &EMOS &1T &3.71$^{+0.10}_{-0.08}$ &&8.0$^{+0.4}_{-0.4}$& 0.49$^{+0.15}_{-0.15}$& 0.48& 0.70$^{+0.11}_{-0.11}$& 0.68$^{+0.05}_{-0.05}$& 366/271 \\
 8.00-13.50 &EMOS &1T &3.75$^{+0.12}_{-0.10}$ &&7.3$^{+0.4}_{-0.4}$& 0.43$^{+0.14}_{-0.13}$& 0.84& 0.62$^{+0.11}_{-0.10}$& 0.57$^{+0.05}_{-0.05}$& 439/325 \\
  8.00-13.50 &EMOS &2T &4.30$^{+1.68}_{-0.29}$ &1.43$^{+0.76}_{-0.21}$  &7.3$^{+0.3}_{-0.4}$& 0.44$^{+0.07}_{-0.13}$& 0.73& 0.65$^{+0.12}_{-0.13}$& 0.53$^{+0.08}_{-0.11}$& 409/322 \\
  8.00-13.50 &EMOS &14T& & &9.3$^{+1.2}_{-1.3}$& 0.33$^{+0.16}_{-0.08}$& 0.78& 0.66$^{+0.09}_{-0.09}$& 0.57$^{+0.04}_{-0.06}$& 396/311 \\
\hline
 0.05- 0.25 &EPN &1T &0.78& &28.8& 0.01& 0.00& 0.09& 0.14& 1151/139 \\
 0.25- 0.50 &EPN &1T &1.37& &12.5& 0.00& 0.00& 0.45& 0.71& 1087/201 \\
 0.50- 1.00 &EPN &1T &1.89& &8.7& 0.04& 0.00& 0.98& 1.48& 1044/343 \\
 1.00- 1.40 &EPN &1T &2.38$^{+0.04}_{-0.04}$ &&7.2$^{+0.6}_{-0.7}$& 0.19$^{+0.15}_{-0.13}$& 0.00& 1.38$^{+0.17}_{-0.13}$& 1.88$^{+0.11}_{-0.08}$& 476/313 \\
 1.40- 2.00 &EPN &1T &2.70$^{+0.04}_{-0.04}$ &&7.2$^{+0.5}_{-0.5}$& 0.25$^{+0.13}_{-0.13}$& 0.08& 1.29$^{+0.14}_{-0.13}$& 1.68$^{+0.08}_{-0.07}$& 459/364 \\
 2.00- 2.80 &EPN &1T &2.92$^{+0.05}_{-0.04}$ &&7.5$^{+0.5}_{-0.6}$& 0.39$^{+0.15}_{-0.13}$& 0.09& 1.00$^{+0.12}_{-0.11}$& 1.49$^{+0.08}_{-0.06}$& 579/412 \\
 2.80- 4.00 &EPN &1T &3.25$^{+0.05}_{-0.05}$ &&7.3$^{+0.5}_{-0.4}$& 0.06$^{+0.11}_{-0.06}$& 0.20& 0.82$^{+0.11}_{-0.11}$& 1.06$^{+0.05}_{-0.05}$& 533/472 \\
 4.00- 5.60 &EPN &1T &3.60$^{+0.06}_{-0.04}$ &&6.6$^{+0.4}_{-0.4}$& 0.12$^{+0.12}_{-0.12}$& 0.01& 0.54$^{+0.12}_{-0.12}$& 0.80$^{+0.04}_{-0.04}$& 591/496 \\
 5.60- 8.00 &EPN &1T &3.84$^{+0.07}_{-0.07}$ &&6.1$^{+0.4}_{-0.4}$& 0.05$^{+0.12}_{-0.05}$& 0.05& 0.40$^{+0.11}_{-0.11}$& 0.65$^{+0.04}_{-0.04}$& 579/527 \\
 8.00-16.00 &EPN &1T &3.98$^{+0.14}_{-0.05}$ &&5.7$^{+0.3}_{-0.5}$& 0.04$^{+0.16}_{-0.04}$& 0.00& 0.36$^{+0.11}_{-0.09}$& 0.63$^{+0.06}_{-0.03}$& 805/687 \\
 8.00-16.00 &EPN &2T &4.14$^{+0.17}_{-0.06}$ &1.06$^{+0.08}_{-0.17}$  &6.2$^{+0.4}_{-0.5}$& 0.24$^{+0.14}_{-0.12}$& 0.01& 0.44$^{+0.11}_{-0.11}$& 0.66$^{+0.05}_{-0.03}$& 746/684 \\
 8.00-16.00 &EPN &14T& & &6.4$^{+3.0}_{-0.4}$& 0.25$^{+0.18}_{-0.13}$& 0.00& 0.45$^{+0.09}_{-0.10}$& 0.66$^{+0.04}_{-0.05}$& 736/674 \\
\hline
\end{tabular}
\end{table*}
\begin{table*}
\caption{Results of spectrum fitting of the deprojected spectra}
 \begin{tabular}[t]{llllllllllr}
 $R$     & &   & kT1    & kT2  & $N_{\rm H}$ & O & Mg & Si  & Fe &  $\chi^2/dof$\\
(arcmin) & &&(keV) & (keV)  &\hspace{-0.3cm} (10$^{20}{\rm \small cm^{-2}}$) & (solar)&  (solar)& (solar)& (solar)& \\\hline
 0.00- 0.50 &EMOS &1T &1.08& &15.9& 0.17& 0.11& 0.35& 0.45& 1111/129 \\
0.00- 0.50 &EMOS &2T & 1.51$^{+0.05}_{-0.07}$ & 0.71$^{+0.01}_{-0.02}$   &11.4$^{+2.4}_{-1.1}$& 0.49$^{+0.18}_{-0.18}$& 0.89& 1.30$^{+0.23}_{-0.30}$& 1.57$^{+0.24}_{-0.28}$& 169/126 \\
 0.00- 0.50 &EMOS &14T& & &11.4$^{+3.7}_{-2.1}$& 0.48$^{+0.25}_{-0.19}$& 0.89& 1.39$^{+0.46}_{-0.33}$& 1.79$^{+0.42}_{-0.34}$& 139/116 \\
 0.00- 0.50 &EPN &1T &0.97& &16.9& 0.14& 0.04& 0.28& 0.38& 1167/176 \\
 0.00- 0.50 &EPN &2T &1.45$^{+0.07}_{-0.08}$ &0.70$^{+0.02}_{-0.02}$  &11.6$^{+1.2}_{-2.4}$& 0.59$^{+0.29}_{-0.19}$& 0.80& 1.52$^{+0.45}_{-0.38}$& 1.85$^{+0.29}_{-0.35}$& 195/173 \\
 0.00- 0.50 &EPN &14T& & &20.8$^{+12.9}_{-7.5}$& 0.71$^{+0.37}_{-0.28}$& 1.39& 2.48$^{+0.74}_{-1.00}$& 3.44$^{+0.74}_{-1.26}$& 170/163 \\
\hline
 0.50- 1.00 &EMOS &1T &1.43& &13.5& 0.49& 0.24& 1.20& 1.17& 354/146 \\
 0.50- 1.00 &EMOS &2T &1.74$^{+0.07}_{-0.03}$ &0.85$^{+0.03}_{-0.04}$  &9.7$^{+1.3}_{-1.6}$& 1.15$^{+0.45}_{-0.30}$& 1.26& 2.79$^{+0.72}_{-0.42}$& 2.71$^{+0.57}_{-0.33}$& 189/143 \\
 0.50- 1.00 &EMOS &14T& & &9.3$^{+1.2}_{-1.6}$& 1.22$^{+0.47}_{-0.33}$& 1.43& 3.06$^{+0.72}_{-0.62}$& 2.93$^{+0.56}_{-0.75}$& 189/133 \\
\hline
 1.00- 2.00 &EMOS &1T &2.30$^{+0.06}_{-0.05}$ &&8.8$^{+0.8}_{-0.8}$& 0.49$^{+0.22}_{-0.20}$& 0.34& 1.83$^{+0.22}_{-0.20}$& 2.22$^{+0.18}_{-0.16}$& 246/212 \\
 1.00- 2.00 &EMOS &2T &2.46$^{+0.25}_{-0.12}$ &1.30$^{+0.31}_{-0.37}$  &8.7$^{+0.8}_{-0.8}$& 0.62$^{+0.24}_{-0.22}$& 0.53& 2.07$^{+0.27}_{-0.25}$& 2.42$^{+0.23}_{-0.20}$& 220/209 \\
 1.00- 2.00 &EMOS &14T& & &8.6$^{+1.0}_{-0.8}$& 0.62$^{+0.25}_{-0.21}$& 0.58& 2.12$^{+0.28}_{-0.26}$& 2.44$^{+0.22}_{-0.21}$& 214/199 \\
\hline
 0.50- 2.00 &EMOS &1T &1.95& &10.2& 0.40& 0.20& 1.42& 1.70& 658/249 \\
 0.50- 2.00 &EMOS &2T &2.20$^{+0.07}_{-0.05}$ &1.00$^{+0.12}_{-0.08}$  &9.0$^{+0.6}_{-0.6}$& 0.78$^{+0.16}_{-0.16}$& 0.79& 2.23$^{+0.20}_{-0.20}$& 2.46$^{+0.16}_{-0.16}$& 339/246 \\
 0.50- 2.00 &EMOS &14T& & &8.9$^{+0.6}_{-0.7}$& 0.78$^{+0.17}_{-0.15}$& 0.80& 2.33$^{+0.21}_{-0.21}$& 2.54$^{+0.16}_{-0.17}$& 322/236 \\
 0.50- 2.00 &EPN &1T &2.10& &7.6& 0.08& 0.00& 1.24& 1.73& 1074/458 \\
 0.50- 2.00 &EPN &2T &2.21$^{+0.03}_{-0.03}$ &0.92$^{+0.05}_{-0.07}$  &7.9$^{+0.5}_{-0.6}$& 0.45$^{+0.13}_{-0.09}$& 0.19& 1.70$^{+0.16}_{-0.10}$& 2.24$^{+0.14}_{-0.07}$& 649/455 \\
 0.50- 2.00 &EPN &14T& & &8.0$^{+0.4}_{-0.5}$& 0.46$^{+0.11}_{-0.10}$& 0.17& 1.68$^{+0.13}_{-0.13}$& 2.14$^{+0.12}_{-0.09}$& 634/445 \\
\hline
 2.00- 4.00 &EMOS &1T &2.94$^{+0.06}_{-0.06}$ &&9.5$^{+0.6}_{-0.5}$& 0.78$^{+0.20}_{-0.19}$& 0.33& 1.42$^{+0.16}_{-0.15}$& 1.72$^{+0.10}_{-0.09}$& 342/294 \\
 2.00- 4.00 &EMOS &2T  &  5.30$^{+4.35}_{-2.14}$ & 2.42$^{+0.31}_{-0.89}$ &9.4$^{+0.6}_{-0.5}$& 0.72$^{+0.19}_{-0.18}$& 0.39& 1.39$^{+0.16}_{-0.15}$& 1.63$^{+0.13}_{-0.11}$& 324/291 \\
 2.00- 4.00 &EMOS &14T& & &9.3$^{+0.9}_{-0.4}$& 0.78$^{+0.20}_{-0.20}$& 0.44& 1.45$^{+0.15}_{-0.18}$& 1.67$^{+0.09}_{-0.12}$& 319/281 \\
 2.00- 4.00 &EPN &1T &2.84$^{+0.05}_{-0.05}$ &&7.7$^{+0.7}_{-0.7}$& 0.26$^{+0.17}_{-0.16}$& 0.22& 1.15$^{+0.17}_{-0.15}$& 1.56$^{+0.09}_{-0.08}$& 491/463 \\
 2.00- 4.00 &EPN &2T & 37$(>5.0)$  &  2.74$^{+0.08}_{-0.07}$ &7.8$^{+0.6}_{-0.8}$& 0.25$^{+0.16}_{-0.15}$& 0.18& 1.13$^{+0.19}_{-0.13}$& 1.54$^{+0.11}_{-0.07}$& 472/460 \\
 2.00- 4.00 &EPN &14T& & &8.3$^{+1.7}_{-0.9}$& 0.34$^{+0.17}_{-0.19}$& 0.19& 1.11$^{+0.18}_{-0.14}$& 1.48$^{+0.10}_{-0.08}$& 479/450 \\

\hline
 4.00- 8.00 &EMOS &1T &3.54$^{+0.11}_{-0.09}$ &&8.9$^{+0.6}_{-0.5}$& 0.43$^{+0.20}_{-0.19}$& 0.34& 0.78$^{+0.15}_{-0.14}$& 0.83$^{+0.07}_{-0.06}$& 391/332 \\
 4.00- 8.00 &EMOS &2T &6.32$^{+7.99}_{-4.15}$ &2.76$^{+0.55}_{-0.58}$  &8.8$^{+0.6}_{-0.6}$& 0.41$^{+0.19}_{-0.18}$& 0.32& 0.76$^{+0.15}_{-0.14}$& 0.80$^{+0.10}_{-0.09}$& 377/329 \\
 4.00- 8.00 &EMOS &14T& & &9.1$^{+1.0}_{-0.7}$& 0.41$^{+0.18}_{-0.18}$& 0.35& 0.78$^{+0.16}_{-0.14}$& 0.80$^{+0.09}_{-0.07}$& 377/319 \\
 4.00- 8.00 &EPN &1T &3.56$^{+0.10}_{-0.10}$ &&6.4$^{+0.8}_{-0.6}$& 0.03$^{+0.20}_{-0.03}$& 0.33& 0.58$^{+0.18}_{-0.17}$& 0.82$^{+0.07}_{-0.06}$& 541/534 \\
 4.00- 8.00 &EPN &2T &3.57$^{+0.12}_{-0.09}$ &0.84$^{+0.53}_{-0.36}$  &6.9$^{+0.8}_{-0.9}$& 0.12$^{+0.27}_{-0.12}$& 0.36& 0.60$^{+0.21}_{-0.16}$& 0.83$^{+0.11}_{-0.06}$& 536/531 \\
 4.00- 8.00 &EPN &14T& & &6.9$^{+1.5}_{-0.9}$& 0.15$^{+0.22}_{-0.15}$& 0.38& 0.62$^{+0.17}_{-0.17}$& 0.82$^{+0.07}_{-0.07}$& 535/521 \\
\hline
 2.00- 8.00 &EMOS &1T &3.26$^{+0.06}_{-0.05}$ &&9.3$^{+0.3}_{-0.3}$& 0.55$^{+0.12}_{-0.12}$& 0.33& 0.99$^{+0.09}_{-0.09}$& 1.14$^{+0.05}_{-0.05}$& 539/387 \\
 2.00- 8.00 &EMOS &2T &6.17$^{+2.56}_{-1.11}$ &2.60$^{+0.28}_{-0.24}$  &9.2$^{+0.3}_{-0.3}$& 0.52$^{+0.11}_{-0.11}$& 0.32& 0.97$^{+0.08}_{-0.08}$& 1.10$^{+0.07}_{-0.06}$& 495/384 \\
 2.00- 8.00 &EMOS &14T& & &9.2$^{+0.6}_{-0.3}$& 0.52$^{+0.13}_{-0.11}$& 0.34& 0.98$^{+0.08}_{-0.09}$& 1.08$^{+0.05}_{-0.05}$& 502/374 \\
 2.00- 8.00 &EPN &1T &3.23$^{+0.08}_{-0.02}$ &&7.1$^{+0.3}_{-0.7}$& 0.13$^{+0.13}_{-0.13}$& 0.28& 0.83$^{+0.17}_{-0.10}$& 1.15$^{+0.06}_{-0.03}$& 825/686 \\
 2.00- 8.00 &EPN &2T &3.18$^{+0.05}_{-0.04}$ &0.86$^{+0.37}_{-0.22}$  &7.6$^{+0.4}_{-0.7}$& 0.19$^{+0.17}_{-0.10}$& 0.27& 0.82$^{+0.15}_{-0.08}$& 1.12$^{+0.07}_{-0.03}$& 809/684 \\
 2.00- 8.00 &EPN &14T& & &7.7$^{+0.7}_{-1.0}$& 0.22$^{+0.13}_{-0.14}$& 0.26& 0.80$^{+0.06}_{-0.09}$& 1.05$^{+0.07}_{-0.04}$& 801/674 \\
\hline

\end{tabular}

\end{table*}

Table 1 and 2 summarize the results.
Even for the deprojected spectra, the single temperature model
is not acceptable at  $R<2'$.
The two-temperature model dramatically reduces  the $\chi^2$, and the multi-temperature
model slightly improves $\chi^2$.
Outside this radius, $\chi^2$ derived from the two- and the multi-temperature
model are slightly smaller than those of the single-temperature model.
Figure 1 shows a representative spectrum for $R$=0.5--2$'$.
Using the two- and the multi-temperature MEKAL model, not only the continuum and
the Fe-L bump, but also the strength of  the Fe-K line is fitted well.
The consistency between the Fe-L and the Fe-K will be discussed in
detail at \S\ref{FeK}.
There remains a residual structure around 1.2--1.5 keV at the Fe-L/Mg-K region.
Therefore, in Table 1 and 2,  we do not show  errors in the  Mg abundances.

\begin{figure*}[]
\resizebox{8.1cm}{!}{\includegraphics{AA1577_figure2a.ps}}
\resizebox{8.1cm}{!}{\includegraphics{AA1577_figure2b.ps}}
\caption{The radial profiles of the temperature and the hydrogen column density.
Dotted and solid lines correspond to the results of the projected
 spectra and the deprojected spectra, respectively.
Black, red and green correspond to the single, two, and the
 multi-temperature MEKAL model, respectively.
The results from the EMOS are shown in diamonds and those from the EPN are
 shown in crosses.
The dashed horizontal line in the profile of the hydrogen column density
 represents the Galactic value.}
\label{ktnh}
\end{figure*}
\begin{figure}
\resizebox{8.1cm}{!}{\includegraphics{AA1577_figure3a.ps}}
\resizebox{8.1cm}{!}{\includegraphics{AA1577_figure3b.ps}}
\resizebox{8.1cm}{!}{\includegraphics{AA1577_figure3c.ps}}
\caption{Radial profiles of the abundances of Fe, Si and O.
The meanings of symbols are the same as those of Figure 2.
The data with a reduced $\chi^2>2$ are not shown.
}
\label{abund}
\end{figure}

The temperature of the ICM decreases  sharply toward the center
(Figure \ref{ktnh}), and
 we need more than two temperature components to fit the deprojected
spectra at the central region.
The observed sharp temperature gradient means that
the single temperature
model is not enough to fit each deprojected spectrum,
even if the ICM is isothermal locally.
In addition, the cluster is not circularly symmetric and
the  cool plume-like structure at the center (Sanders \&
Fabian 2002) might introduce an additional temperature
component.

 The hydrogen column density, ${\rm {N_H}}$ is  consistent with the
Galactic value  at $R>1'$,  although the EPN and the
EMOS give slightly different results by a few times $10^{20}{\rm
cm^{-2}}$ (Figure \ref{ktnh}).
Within $R<1'$,  the two- and the multi-temperature models give similar
values to those of $R>1'$.
Higher column densities derived from the single
temperature model fit within $R<1'$ are not acceptable due to their high $\chi^2$.
Therefore,  ${\rm {N_H}}$ is consistent with the Galactic value within the whole field of view.

 Discarding the results  of  unacceptable fits (reduced $\chi^2>2$),
 the  Fe abundance is $\sim$0.6 solar  at $R>8'$ and
  within the radius, it increases steeply toward center.
Within $2'$, the gradient becomes weaker.
The average value of the Fe abundance at $R<2'$ is 2.3 solar  (Figure \ref{abund}).
The EPN and the EMOS give  consistent Fe abundances within 10\% (Table 2).
The Fe abundances from  the deprojected spectra are slightly
higher than those from the projected spectra.

 At each radius, the Si abundance
 is close to the Fe abundance (Figure \ref{abund}, \ref{abund_ratio}).
The uncertainties in the Si/Fe ratio are better constrained than those in the Si and
 Fe abundances themselves (\ref{abund_ratio}), since the derived abundance of  Si and Fe
are correlated to each other.
On average, the Si/Fe ratio is 0.89$\pm$0.04  and 0.75$\pm$0.04 in units of the solar
 ratio using the EMOS and EPN, respectively.

\begin{figure}[]
\centerline{\resizebox{8.1cm}{!}{\includegraphics{AA1577_figure4.ps}}}
\caption{Radial profiles of the O/Fe (black lines) and the Si/Fe
 (gray lines)  ratios in units of the
 solar elemental ratio derived from the multi-temperature MEKAL model of  the EMOS
 (diamonds) and the EPN (crosses) spectra.
}
\label{abund_ratio}
\end{figure}

 The O abundances are much smaller than the Si and Fe abundances
(Figure \ref{abund}, 4).
 The two detectors give inconsistent O abundances.
Using the EMOS,
the O abundance is about 0.8 solar at $R$=0.5--2.0$'$ and at $R>$2$'$,
it reduces to 0.4 solar (Figure \ref{abund}),
and the O/Fe ratio increases toward outer regions (Figure \ref{abund_ratio}).
In contrast, the EPN gives a significantly  smaller O
abundance than the EMOS especially in the outer regions (Figure \ref{abund}),
and the profile of the  O/Fe ratio is consistent with no radial gradient
(Figure \ref{abund_ratio}).

In summary, as in center of other clusters and groups of galaxies,
the Fe and Si abundances are close to  each other with strong negative radial
gradients.
The O abundance is at least a factor of 2 smaller.
 The discrepancies in the O and Si abundances between the EMOS and
EPN will be discussed in section 4.3.
\section{Uncertainties in the abundance determination}

 In the abundance determination, we must examine uncertainties such as the
dependence on the plasma code and on the background subtraction.
In this section, we study these uncertainties and also calibrate the
abundances with the strengths of the lines.

\subsection{The effect of the plasma code}

In order to constrain the effect of the plasma code on the abundance determination,
  we compared the results from the APEC (Smith et al. 2001) model with those
from the MEKAL model.
We  used the APEC version 1.1  model in XSPEC version 11.2.
As in the MEKAL model fit, we fitted the deprojected spectra with a single,
and  a multi-temperature APEC model.

The results are summarized in Table 3.
With the APEC model, the fit to the Fe-L/Mg-K region at 1.2--1.5 keV
improved  from that with the MEKAL code (Figure 1).
As a result, the reduced $\chi^2$ are consistent or  slightly smaller
than those from the MEKAL model fit.
The derived temperatures, hydrogen column densities, and
the  Si and Fe abundances are consistent within 10\% with those
from the MEKAL code (Figure \ref{apec_fe}, \ref{apec_all}).

However, the O and the Mg abundances increased by $\sim$20\% and$\sim80$\%,
 respectively,   from the MEKAL model fit.
The difference in the O abundance is consistent with the difference of the
 strength of the H-like O line between the APEC and MEKAL models,
since at 2 keV, that of APEC is 10\% larger than that of MEKAL model,
and at 4 keV, the difference increases to 30\%.
The difference in the  Mg abundance is not due to the difference in
the strength of the Mg-K line between the two codes  which is smaller than that of O below 4 keV.
It should be caused by the difference in the Fe-L modeling around the Mg-K line.
We will discuss it later in \S4.3.2.

\begin{table*}
\caption{Results of spectrum fitting of the deprojected spectra within
 8$'$ and projected spectrum at 8--13.5$'$ of the EMOS with the
 single- and the multi-temperature APEC model.}
 \begin{tabular}[t]{lllllllllr}
 $R$     &  &  & kT    & $N_{\rm H}$ & O & Mg & Si  & Fe &  $\chi^2/dof$\\
(arcmin) & &&(keV)   & (10$^{20}{\rm cm^{-2}}$) & (solar)&
  (solar)& (solar)& (solar)& \\
 \hline
 0.00- 0.50 &EMOS &1T &1.00 &17.1& 0.36& 0.23& 0.39& 0.27& 676/129 \\
 0.00- 0.50 &EMOS &14T& & 10.6$^{+2.7}_{-1.5}$& 0.50$^{+0.23}_{-0.21}$& 1.45$^{+0.49}_{-0.49}$& 1.47$^{+0.34}_{-0.40}$& 1.72$^{+0.19}_{-0.36}$& 146/116 \\
\hline
 0.50- 2.00 &EMOS &1T &1.93 &11.1& 0.47& 0.68& 1.35& 1.61& 585/249 \\
 0.50- 2.00 &EMOS &14T&  &9.3$^{+0.6}_{-0.7}$& 0.91$^{+0.21}_{-0.19}$& 1.54$^{+0.15}_{-0.24}$& 2.29$^{+0.25}_{-0.20}$& 2.42$^{+0.20}_{-0.16}$& 266/236 \\
\hline
 2.00- 4.00 &EMOS &1T &2.94$^{+0.06}_{-0.06}$ &9.8$^{+0.6}_{-0.5}$&
  0.96$^{+0.27}_{-0.25}$& 0.89$^{+0.28}_{-0.27}$&
  1.46$^{+0.17}_{-0.16}$& 1.83$^{+0.11}_{-0.10}$& 346/294 \\
 2.00- 4.00 &EMOS &14T&  &9.5$^{+0.7}_{-0.6}$& 1.00$^{+0.26}_{-0.25}$& 0.89$^{+0.28}_{-0.25}$& 1.49$^{+0.19}_{-0.16}$& 1.76$^{+0.13}_{-0.12}$& 301/281 \\
\hline
 4.00- 8.00 &EMOS &1T &3.53$^{+0.11}_{-0.11}$ &9.1$^{+0.6}_{-0.5}$& 0.61$^{+0.27}_{-0.26}$& 0.62$^{+0.31}_{-0.30}$& 0.84$^{+0.16}_{-0.16}$& 0.92$^{+0.08}_{-0.08}$& 397/332 \\
 4.00- 8.00 &EMOS &14T&  &9.1$^{+0.5}_{-0.7}$& 0.54$^{+0.27}_{-0.23}$& 0.58$^{+0.32}_{-0.28}$& 0.84$^{+0.18}_{-0.15}$& 0.88$^{+0.10}_{-0.08}$& 372/319 \\
\hline
 8.00-13.50 &EMOS &1T &3.77$^{+0.10}_{-0.10}$ &7.4$^{+0.4}_{-0.4}$&  0.52$^{+0.18}_{-0.18}$& & 0.67$^{+0.12}_{-0.11}$& 0.63$^{+0.06}_{-0.06}$& 443/325 \\
 8.00-13.50 &EMOS &14T& & 8.7$^{+1.1}_{-1.1}$& 0.38$^{+0.18}_{-0.16}$& & 0.72$^{+0.13}_{-0.12}$& 0.60$^{+0.08}_{-0.07}$& 388/312 \\
\hline
\end{tabular}

\end{table*}

\begin{figure}[]
\resizebox{8.1cm}{!}{\includegraphics{AA1577_figure5.ps}}
\caption{The Fe abundance profile derived from the MEKAL (gray data) and the APEC
 (black data) model, from the single-temperature model (crosses)
 and the multi-temperature model (diamonds).The data with a reduced $\chi^2>2$ are not shown.}
\label{apec_fe}
\end{figure}
\begin{figure}[]
\resizebox{8.1cm}{!}{\includegraphics{AA1577_figure6.ps}}
\caption{ The ratio of the O(open triangles), Mg(crosses), Si(open
 circles) and Fe(closed circles) abundances and the reduced $\chi^2$
(closed boxes) between the multi-temperature APEC and the multi-temperature MEKAL model.
}
\label{apec_all}
\end{figure}

\subsection{Effect of the  background uncertainty}

 One of the most severe problems in analyzing  XMM-Newton data
are uncertainties in the background.
In this paper, we adopted  deep survey data as a background, which
agree well with the data of the Centaurus cluster above 8 keV (Figure \ref{mos_spec_bgd}).
In addition, in order to study the effect of the uncertainty of the background, we
artificially scaled  the background by 10\%, and
fitted the projected EMOS spectra at $r>2'$ in the same way as previously.
Since spectral variations of the  background amount to about 10\% below 1 keV
when the background is scaled with the count-rate outside the field of
the view of the detector (Katayama et al. 2004), and
the relatively high  Galactic $N_{\rm H}$
towards the Centaurus cluster absorbs the low energy photons from the
Cosmic X-ray Background (CXB).

The results are summarized in Figure \ref{bgd}.
Within 8$'$, the derived temperatures, the Fe abundances, the O/Fe and
the Si/Fe ratios are consistent within a few \% with those derived from
the background used in \S3.1.
Outside 8$'$, the 10\% change of the background changes derived
parameters by $\sim$ 10\%.
Therefore,  the background problem is not severe in this observation.

\begin{figure}[]
\resizebox{8.1cm}{!}{\includegraphics{AA1577_figure7.ps}}
\caption{The raw EMOS spectrum at $r>8'$ (black crosses) and
the adopted background spectrum (black diamonds), and the background
 subtracted spectrum (gray crosses).
}
\label{mos_spec_bgd}
\end{figure}

\begin{figure}[]
\resizebox{8.1cm}{!}{\includegraphics{AA1577_figure8.ps}}
\caption{
The ratio of derived parameters of the projected EMOS spectra with the
 multi-temperature  model using a  background scaled by a factor of 1.1
to those using the unscaled background used in the paper.
}
\label{bgd}
\end{figure}

\subsection{Comparisons between the line strength and model fit}
\subsubsection{The line strengths of O and Si and the abundance determination}

In order to study the discrepancy in the O and the Si abundances
between the EMOS and the EPN data,  it is important to check their line strengths directly.
Complications arise
since the energy resolution of the EMOS has become worse due to the
radiation damage in orbit (Kirsh 2002),
 and that of the EPN depends on the distance from the
read-out.
In addition, there are still discrepancies of several \% in the
response matrix between the EPN and EMOS,
 which might give a large uncertainty in strengths of weak lines.

\begin{figure}
 \centerline{
\resizebox{4.1cm}{5.5cm}{\includegraphics{AA1577_figure9a.ps}}
\resizebox{3.9cm}{5.5cm}{\includegraphics{AA1577_figure9b.ps}}
}
\caption{
Deprojected spectra of the EMOS (EMOS1+EMOS2; lower curve) and the
 EPN (upper curve) at $R$=2.0--8.0$'$  around
the energy of  the lines of O (left panel) and Si (right panel).
The gray data points and black solid lines
 correspond to the best fit model with one temperature MEKAL model and
that with Gaussians with 0 line widths, respectively.  The black dotted lines represent
the continuum emissions as described by the Gaussian fit.
}
\label{osiline}
\end{figure}

\begin{figure}[]
\centerline{
\resizebox{8.1cm}{6cm}{\includegraphics{AA1577_figure10.ps}}
}
\caption{The ratio of line strengths K$\alpha$ of H-like O (upper panel) and Si (lower panel)
 derived from the Gaussian fit to those of best fit values from spectral fit for the EMOS (black lines)
and EPN (gray lines).
Crosses and diamonds correspond to the fitting with a Gaussian with 0 line width and free line width, respectively.
Errors correspond the 68\% level.
}
\label{eqw}
\end{figure}

The  strengths of K$\alpha$ lines of H-like O and Si are derived
 from fittings of the spectra around the lines with Gaussians. The details are
the same as in Matsushita et al. (2003).
First, the line widths of the Gaussians were frozen to  zero, and then
allowed to be free.
Figure \ref{osiline} compares the best fit
MEKAL model and the Gaussian fits for  representative spectra at
$R$=2--8'.
In the EMOS spectrum, we can see a weak bump of the H-like O line, and a clear
bump of the H-like Si line.
In contrast, in the spectrum of the EPN, which has an  energy resolution
 worse than that of
the EMOS, the continuum and the O line are hardly
distinguished and the  Si line is much broader than the EMOS one.

For the EMOS spectra, the line strengths of K$_\alpha$ of H-like O and
Si from the Gaussian fits are consistent within 10\%
with the those from the MEKAL model, except for the O line strength within
0.5$'$, where the O line is completely hidden in the Fe-L lines (Figure \ref{eqw}).
This result indicates that the effect of the decrease of the energy resolution of the EMOS detector
should not affect  the derived O and Si abundances.

In contrast,
allowing the line width to be a free parameter,
the Gaussian fits to the EPN spectra give systematically larger line
strengths than the MEKAL model fit.
As a result, adopting the values from the Gaussian fits,
the EPN abundances become consistent with the EMOS ones.
 Therefore,
the O and Si abundances derived from the EMOS fit should be reliable,
since it has a better spectral resolution and it gives consistent
 strengths of the K$\alpha$ lines between the Gaussian fits and the
 MEKAL model fits.

\begin{figure}[]
\centerline{
\resizebox{8.1cm}{6cm}{\includegraphics{AA1577_figure11.ps}}
}
\caption{The line ratios of K$\alpha$ lines of H-like O and Si of the
projected spectra of the EMOS, plotted
 against  the best fit temperature fitted with the single MEKAL model.
Dashed lines  correspond to constant abundance
 ratios in units of the solar ratio.
Errors represent the 68\% confidence level.
}
\label{osiratio}
\end{figure}

As shown in the Figure \ref{osiratio},
the ratio of strengths of K$\alpha$ lines of H-like O and Si becomes constant above
1.7 keV and increases toward lower energies.
This temperature dependence means that
any temperature distribution cannot yield a  O/Si ratio larger than 0.6 solar within 4$'$.
Furthermore, we got a higher value of the line ratio at $R>8'$ by a factor of
2.
It implies that the O/Si ratio increases  in the region, since
the contribution to the O line from the component below 1.7 keV of the
multi-temperature MEKAL model is smaller than 10\%.

\subsubsection{The line strength of the Mg-K}

It is also important to  derive the strengths of the K$\alpha$-lines of
Mg  directly, since the Mg abundances
derived from the spectral fits depend on the modeling of the underlying Fe-L
lines. We therefore fitted the EMOS spectra within  the  energy range of 1.3--1.65 keV
with Gaussians plus one- two- or three-temperature MEKAL or APEC model.

 All of  the Gaussian models can fit the spectra around the
Mg-K/Fe-L  region well (Figure \ref{mgkspec}).
The derived  strengths of the K$\alpha$-line of H-like and He-like Mg
do not depend on the temperature structure (i.e. one-, two, or
three-temperature model) or the  plasma code (i.e. MEKAL or APEC
model).
The line strengths agree well with those  derived from the fitting
the spectra
 described in \S4.1, but are systematically higher than those derived
from the multi-temperature MEKAL model described in \S3,
which cannot reproduce the spectra around the Mg-K/Fe-L region (Figure \ref{mgline}).
Therefore, it is reasonable to adopt the Mg abundances derived
from the multi-temperature APEC model fit as the Mg abundances of the ICM.

\begin{figure}[]
\centerline{
\resizebox{8.1cm}{6cm}{\includegraphics{AA1577_figure12.ps}}
}
\caption{
The deprojected  spectrum  of the EMOS at $R$=0.5--2.0$'$ (black closed circles)
fitted with the multi-temperature MEKAL model (green closed circles),
the multi-temperature APEC model (red closed circles),
the Gaussians with MEKAL models (green dashed lines) and the Gaussians
with the APEC models (red dashed lines).
The contributions of the continuum plus the Fe-L are also shown for the
multi-temperature APEC model (red open circles) and the
 multi-temperature MEKAL model (green open circles) and the Gaussian fit
(red and green dashed lines).
}
\label{mgkspec}
\end{figure}

 We  note that  the Mg/O ratio  does not depend on the temperature structure
since the line ratio of K$\alpha$ lines of these two elements is nearly
 constant above 1.1 keV (Matsushita et al. 2003).

\begin{figure}[]
\centerline{
\resizebox{8.1cm}{6cm}{\includegraphics{AA1577_figure13.ps}}
}
\caption{
The profile of the line strengths of the K$\alpha$-line of He-like
and H-like Mg of the best fit model of the multi-temperature model (horizontal solid
 lines) and derived from the Gaussians plus a single temperature model
(solid diamonds), two temperature model (dashed diamonds), and
 three-temperature model (dotted diamonds).
The gray and black data correspond to the MEKAL and APEC model,
 respectively.
Errors correspond the  68\% confidence level.
}
\label{mgline}
\end{figure}

\subsubsection{The line strength of Fe-K}\label{FeK}

Since the temperature dependence  of the intensities of the Fe-L and Fe-K lines
is completely different,  a comparison between the Fe-L and the Fe-K
lines  strongly constrains
the temperature structure and the Fe abundance.
In the spectral fitting by the MEKAL  model or the APEC model,
the strengths of the 6.7 keV Fe-K lines are fitted well, although the
fit to the Fe-L lines mostly determines the Fe abundance due to its high
statistics (Figure \ref{fechi}).

When the Fe abundance is shifted by 40\% in the fits
 with the multi-temperature model,
the Fe-L structure can  be roughly fitted  although the $\chi^2$
increased significantly (Figure \ref{fechi}).
However,
the strengths of the Fe-K line cannot be reproduced.
Therefore, the uncertainties in the Fe-L line fit, due to the temperature structure and
the plasma code should not be  severe problems at least in the Centaurus cluster.

\begin{figure}[]
\centerline{
\resizebox{8.1cm}{6cm}{\includegraphics{AA1577_figure14.ps}}
}
\caption{The  $\chi$ distributions of the deprojected spectrum at
 $R$=0.5--2.0$'$ fitted with the multi-temperature APEC model.
The solid black line corresponds to the best fit model, and the dotted black
 line and dashed gray lines correspond to the model where the Fe
 abundance is fixed to be 1.6 solar and 3.2 solar, respectively.
}
\label{fechi}
\end{figure}

Since abundances derived from the Fe-K line may have an uncertainty
due to the uncertainty of the background,
we have also derived the line strength of the Fe-K line directly from a
Gaussian fit.
The width of the Gaussian was allowed to be a free parameter,
since the 6.7 keV Fe-K consists of several strong lines.
In figure \ref{fek}, the derived line strengths from the Gaussian fit are compared to the
line strengths of the Fe-K line derived from the best fit
multi-temperature MEKAL model.
These values agree  within 10\%.
Thus,  the line strengths of the Fe-K line are consistent with the Fe
abundances derived from the MEKAL  model fit and a change of the Fe
abundance cannot reproduce the  observed line strength of the Fe-K.

\begin{figure}[]
\centerline{
\resizebox{8.1cm}{6cm}{\includegraphics{AA1577_figure15.ps}}
}
\caption{ The ratio of line strengths of the 6.7 keV Fe-K line
 derived from the Gaussian fit to those of best fit values from spectral
 fit for the EMOS (black lines) and EPN (gray lines), where the Fe-L is
 important to determine the Fe abundance.
Errors correspond to the 68\% level.
}
\label{fek}
\end{figure}

\section{Discussion}

\subsection{Summary of the results}

The abundances of O, Mg, Si, and Fe in the ICM of the Centaurus cluster are derived.
  We have checked uncertainties in the temperature structure,
 in the background subtraction, and in the spectral model and
studied their effects on the abundance determination.
The Fe abundance is $\sim2.3$ solar within 2$'$ and decreases to
$\sim$0.6 solar at $R>8'$.
The Si abundance is close to the Fe abundance.
In contrast, the  O and Mg abundances  are  much  smaller than
the Fe and Si abundances in units of the solar ratio.

The abundance pattern of the ICM of the Centaurus cluster, the low O abundance compared to those
of  Si and Fe, resembles to those observed in center of other clusters
and groups of galaxies, such as M 87 (Matsushita et al. 2003), A496 (Tamura et al. 2001b),
Fornax cluster (Buote et al. 2002) and
group-center elliptical galaxies NGC 4636 (Xu et al. 2002), NGC 5044 (Tamura
et al. 2003;  Boute et al. 2003).
However, there are small differences in the observed abundance pattern of the ICM.
For example,
the central Fe abundance of the Centaurus cluster (2.3 solar) is 40\%
larger than
that of M 87 (1.6 solar). In addition, the Si/Fe ratio of the former is 20\% smaller than that
of the latter.
 In this section, we mainly compare and discuss the abundance pattern of the Centaurus
clusters with that of M 87, since
these two clusters are the nearest and the best studied objects among
relatively low temperature clusters.

\subsection{Comparison with stellar metallicity and SN II abundance pattern}
The O and Mg in the gas around a cD galaxy is a mixture of those in the
ICM and those in the accumulation of  stellar mass loss from the cD
galaxy, since these elements are only synthesized by SN II.
The O and Mg abundances of the mass loss  reflect those of mass losing stars,
which contribute significantly to the optical light from elliptical galaxies.
The stellar metallicity of elliptical galaxies are usually derived
from the Mg$_2$ index in the optical spectra,
which  depends mainly on the Mg abundance and stellar metallicity
where O contributes most, and weakly on the age population of stars.
Therefore, comparing the O and Mg abundances of the gas and stellar
metallicity derived from the optical Mg$_2$ index is important to study
the gas flow and contribution of stellar mass loss, and stellar metallicity
of the cD galaxies.

\begin{figure}[]
\centerline{
\resizebox{8.1cm}{6cm}{\includegraphics{AA1577_figure16.ps}}}
\caption{ Mg (closed circles) and O (diamonds) abundances derived
for the Centaurus cluster (black) and M 87 (gray)
 from the multi-temperature MEKAL (dotted lines) and APEC (solid lines)  model.
The dashed lines represent the stellar metallicity of  NGC 4696
 (black) and M 87 (gray)  derived from the optical Mg$_2$ index (Kobayashi \& Arimoto 1999).
}
\label{mgo}
\end{figure}

The Mg abundances of the two clusters are close to  their stellar metallicity derived
from the Mg$_2$ index  (Figure \ref{mgo}; Kobayashi \& Arimoto 1999).
 The gradient of the Mg abundance of the gas around M 87 is steeper than in the Centaurus
cluster. At a radius of 10--20 kpc,  the Mg abundance of the
Centaurus cluster is a factor of 2 larger than that of M 87 (Figure \ref{mgo}).
The stellar metallicity gradient of  M 87 is also steeper than that of
NGC 4696, the cD galaxy of the Centaurus cluster.
The agreements of between the Mg abundances with
stellar metallicity  at the central regions indicates that in these
regions, the gas  is  dominated by gas ejected from the cD galaxies.

The Mg/O ratio of the gas of the Centaurus cluster
 is 1.2 $\pm$ 0.3 of the solar ratio on average as determined with the
 multi-temperature APEC model.
This value is close to  that of the ICM within 4$'$ of
  M 87, which is  1.3$\pm$ 0.1  solar ratio (Matsushita et al. 2003),  and
also to the value of 1.3$\pm 0.2$ solar ratio of NGC 4636 (Xu et al. 2003) derived from the RGS.
The observed Mg/O ratios of the gas at the cluster centers
are  close to [Mg/O] of the Galactic stars (Edvardsson et al. 1993).
Therefore, at least for the Mg/O ratio, the Galactic SN II and
those trapped in stars in the cD galaxies have no difference.

\subsection{The Fe abundance profile and SN Ia contribution}

\begin{figure}[]
\centerline{
\resizebox{8cm}{!}{\includegraphics{AA1577_figure17.ps}}}
\caption{The Fe abundance of the ICM of the center of Centaurus
 cluster (black) and M 87 (gray). }
\label{mgas0}
\end{figure}

The Fe in the gas at the core of clusters is also a mixture of those in the ICM and the recent
supply from the cD galaxy.
The latter contains Fe synthesized by SN Ia  and  those coming from
stars  through stellar mass loss, since Fe is synthesized by both SN Ia
and SN II.

The Fe abundance of the ICM of the Centaurus cluster is systematically
higher than that around M 87 at a same distance from the cluster center
(Figure \ref{mgas0}).
The peak  Fe abundance of the Centaurus cluster is 2.3 solar.
This value is significantly higher than that of  M 87, which is 1.6 solar.
Assuming that the O/Fe ratio of SN II is 3,
 the central Fe abundances from SN Ia of the Centaurus cluster and M 87
become 2 and 1.3 solar, respectively.
 Since the SN Ia contribution to the Fe abundance is dominant, the
uncertainty in the assumption for the O/Fe ratio does not change the result very much.

\begin{figure}[]
\centerline{\resizebox{8.1cm}{!}{\includegraphics{AA1577_figure18.ps}}
}
\caption{The Fe abundance (the upper panel) and   $\rm{(Fe/Si)}_{\rm{SN Ia}}$ (the middle and the bottom panel)
in units of the solar values are
plotted against the ratio of the Fe mass to B-band luminosity  of the cD galaxy (IMLR),
for M 87 (gray circles) and the Centaurus cluster (black circles), when adopting the abundance pattern
of SN II from the average value of Galactic metal poor stars (the middle panel; Clementini et al. 1999) and from
nucleosynthesis model (the bottom panel) by Nomoto et al. (1997) assuming Salpeter's initial mass function (Iwamoto et al. 1999). }
\label{mgas}
\end{figure}

The Fe abundance of gas from SN Ia in an elliptical galaxy is
proportional to $M^{\rm Fe}_{\rm SN} \theta_{\rm SN}/\alpha_*$(see
Matsushita et al. 2003 for details).
Here,  $M^{\rm Fe}_{\rm SN}$ is the mass of Fe synthesized by one SN Ia,
$\theta_{\rm SN}$ is SN Ia rate, and $\alpha_*$ is stellar mass loss rate.
 The higher Fe abundance of the gas in  the central region of the
Centaurus cluster indicates a higher $M^{\rm Fe}_{\rm SN} \theta_{\rm SN}/\alpha_*$.
 The cooling flow rate derived from the standard cooling flow model
is higher in the Centaurus cluster (Allen \& Fabian 1994) than that of the M 87 (Matsushita
et al. 2002).
 B\"ohringer et al. (2004)  questioned the standard cooling flow
model comparing the Fe mass profile of 4 clusters of
galaxies with cooling cores including M 87 and the Centaurus cluster.
They concluded that we need long enrichment times ($>5$ Gyr) in order to
accumulate the observed Fe abundance peak even if the SN Ia rate was
larger in the past.

As shown in Figure 18, a difference between M 87 and the Centaurus cluster is
the ratio of the  Fe mass to the stellar B-band luminosity  of the cD
galaxy(IMLR).
The total B-band luminosity and the effective radius were calculated
using Prugniel and Heraudeau (1998), and the effect of the Galactic extinction
was corrected using Schlegel et al. (1998).
The IMLR of the Centaurus cluster is much higher than that of the M 87,
especially within the central region.
Since the contribution of the SN Ia to  Fe in the ICM is dominant,
this indicates that accumulation time scale of SN Ia is higher in the
Centaurus cluster than that in M 87,
although we do not know the actual gas flow
rate due to the cooling flow problem.
The longer accumulation time scale in the Centaurus cluster means
that  $M^{\rm Fe}_{\rm SN} \theta_{\rm SN}/\alpha_*$  was higher in the past.
In other words,  the Fe mass synthesized by a SN Ia was higher in the past or
the ratio of SN Ia rate to stellar mass loss rate was higher in the past
as suggested in Renzini et al. (1993).

\subsection{Abundance pattern of SN Ia }

 Si is both synthesized by SN Ia and SN II, and the abundance
pattern of  O, Si, and Fe strongly constrains the nucleosynthesis  of the
SN Ia when Fe is dominated by SN Ia.
  Figure \ref{osife} summarizes the  ratio of these three elements in the ICM
       of the Centaurus cluster and     M 87 (Matsushita et al. 2003).
   As in M 87, the data of the Centaurus cluster cannot be explained by
       a sum of SN II abundance pattern in the Galactic metal poor stars (Clementini
       et al. 1999), and SN Ia
       abundance pattern by the W7 model.   The Si abundances are clearly higher than
       the sum of the two.

 At the cluster center, the Fe/Si ratio and the Fe/O
ratio of the gas of the Centaurus cluster are systematically higher than
those of M87, respectively.
       The main difference between M 87 and the Centaurus Cluster is the
       IMLR as described in the previous section.
       In figure \ref{mgas},  $ \rm{(Fe/Si)}_{\rm{SN Ia}}$ is also
       plotted against IMLR.
The derived  $ \rm{(Fe/Si)}_{\rm{SN Ia}}$ value is much smaller  than the
       value of 2.6 in units of the solar ratio which is
       predicted by the W7 model.
Regions with larger IMLR have
       larger values of  $\rm{(Fe/Si)}_{\rm{SN Ia}}$, when
   adopting the SN II pattern of either the Galactic stars
       (Clementini et al. 1999), or the
       nucleosynthesis model (Iwamoto et al. 1999),
         A  larger  IMLR corresponds to a longer accumulation time scale.
       For  M 87, it needs only a few Gyr to accumulate the observed gas
      mass within 10kpc where the gas from the cD galaxy is dominant (Matsushita et al. 2002).
       In contrast, in the center of the Centaurus cluster,
         ejecta of SN Ia are accumulated over a  much longer time scale than
      that of M 87.
     Therefore, the correlation between  $\rm{(Fe/Si)}_{\rm{SN Ia}}$ and IMLR
     support the suggestion  by Finoguenov et al (2002) and Matsushita
       et al. (2003) from the M 87 observation
     that  $ \rm{(Fe/Si)}_{\rm{SN Ia}}$ depends on the age of the system.
 Matsushita et al. (2003) discovered
that the Si/O ratio of the Galaxy also increases  systematically toward metal rich stars.
This result indicates that there is a source of high Si/O ratio in our
Galaxy at present and supports the scenario suggesting a  dependency of the Fe/Si ratio of
ejecta of SN Ia on the age of the system.

\begin{figure}[]
\centerline{
\resizebox{8.1cm}{!}{\includegraphics{AA1577_figure19.ps}}
}
\caption{[Fe/Si] of the ICM of the Centaurus cluster (diamonds) and M 87
 (crosses; Matsushita et al. 2003) are plotted against [Fe/O].
The average value of Galactic metal poor stars (Clementini et al. 1999;
 open square)  and  the abundance ratio of SN II model using the
 nucleosynthesis model (asterisk) derived in Nomoto et al. (1997), assuming
 Salpeter's IMF (Iwamoto et al. 1999) are shown.
 The solid line and
 dashed line represent the relation of the abundance pattern synthesized by
 SN Ia with Fe/Si=1.1 (the best fit relation of M 87) and Fe/Si=2.6 (W7 ratio;
 Nomoto et al. 1984), respectively.
}
\label{osife}
\end{figure}

\subsection{The hydrogen column density and the cooling flow model}

In the ASCA era, in order to explain observed  fluxes of soft energy
photons which are much smaller than the expected value from the standard
cooling flow model,  absorption  within cluster cores was discussed
(Allen et al. 2001).
In order to obscure a cooling flow in the Centaurus cluster from the standard model,
we need at least additional column density around $2\times
10^{21}\rm{cm^{-2}}$.
However, with the XMM-Newton observations,  the observed hydrogen column
density  is too low to conceal the cool component from the cooling flow model
(Matsushita et al. 2002, B\"ohringer et al. 2002).
The observed hydrogen column density of the Centaurus cluster is also consistent
with the Galactic value, $8.06\times 10^{20}\rm{cm^{-2}}$ over the
whole field of view.
This means that  the soft energy photons from the Centaurus cluster are not obscured.

\section{Conclusion}

With the XMM-Newton observation,  the abundance pattern of O, Mg, Si, and Fe of the ICM of the
Centaurus cluster are derived.
 At the very center, the Mg and O abundances are close to the stellar
 metallicity.
This result indicates that the gas at the very center is dominated by
the supply of the stellar mass loss from the cD galaxy.

The abundances of Si and Fe are close to each other in units of the solar
abundance, while the O and Mg abundances are smaller, like in the centers of
other clusters and groups of galaxies.
In order to explain the abundance pattern, the SN Ia ejecta from the cD
galaxy should have a higher Si/Fe ratio than the standard W7 model by Nomoto et
al. (1984).

There are small differences in the Fe abundances and the Fe/Si ratio
in the ICM between the Centaurus cluster and M 87 (Matsushita et
al. 2003). These differences and   the higher IMLR in the
Centaurus cluster may reflect a higher accumulation time scale of SN
Ia.  In order to confirm this  suspicion, we will further study
abundance patterns of the ICM of number of clusters and groups of
galaxies
with Suzaku which has a better energy resolution at the O lines.

\begin{acknowledgements}

 This work was supported by Humboldt foundation.
 The paper is based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions direct
by funded by ESA Member States and the USA (NASA).
 The XMM-Newton project is supported by the Bundesministerium f\"ur Bildung und Forschung, Deutsches Zentrum  f\"ur Luft und Raumfahrt (BMBF/DLR), the Max-Planck Society and the Haidenhain-Stiftung.

\end{acknowledgements}

redpajama_set_name: RedPajamaArXiv


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