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Home News Italy's draft Stability Law could introduce gaming tax reforms
Italy's draft Stability Law could introduce gaming tax reforms
9. December 2015 | Fonte: World Online Gambling Law Report
The draft Stability Law 2016 was proposed this month in Italy and was accompanied by long-awaited tenders including for 80 new online licences. Stefano Sbordoni, Founding Partner at Studio Legale Sbordoni, discusses the draft, as well as the implications of the Customs and Monopolies Agency's recent 'Measures on gaming matters' document and its recommendations.
The Stability Law 2015 (Law no. 190 dated 23 December 2014) entered into force on 1 January 2015 and is aimed at protecting public order and safety, as well as children and weaker members of society. Commencing from 1 January 2015, this marked the start in Italy of a procedure to legalise the position of those parties active as of 30 October 2014 that, on any basis, collect bets and pay cash winnings in Italy, either on their own accounts or on behalf of third parties, including those domiciled abroad, without being connected to the National Totaliser operated by the Customs and Monopolies Agency. This procedure involved such operators making an application by the end of January, and committing to sign a related agreement by 28 February. However, an operator can only collect bets following payment of the flat tax levied pursuant to Decree no. 504 dated 23 December 1998 and its subsequent amendments, which was due for the tax years prior to 2015 that had not yet been closed for tax inspection purposes. This tax would be paid by the shop manager or the gaming operator.
Upon application, the owner of the business or betting shop was granted the right, until expiry of the current Government licences for the collecting of bets to manage gaming income of this type even on behalf of an existing concession holder.
This procedure resulted in the emergence of new betting shops in Italy. In a market that was already saturated, the legalisation of new betting shops made existing operators even more unhappy. Some licensees strengthened their positions by acquiring new betting shops, but the damage caused to small bookmakers was undoubtedly considerable.
The licences will expire on 30 June 2016 and the Government announced its long-awaited call for tenders alongside the draft of the Stability Law 2016, in October 2015. The call will include the renewal of the call for bingo tenders, cancelled back in October 2014, with operators at present continuing in business on the basis of a de facto extension, which does not fully legitimise such activities. The new draft of the Stability Law, which is still to be approved by the Parliament, provides for:
a) a new tender for 15,000 land based licences, and for 7,000 shops where only a corner of the shop is dedicated to gaming. The tender should be held on 31 July 2016;
b) a new tender for 80 new online licences on 31 July 2016;
c) a new tender for 250 bingo licences.
It seems like, with the New Year approaching, the public gaming sector in Italy can expect a season packed with reforms. Indeed, there are some signs that leave room for hope.
The failure to implement a framework for tax reforms has undoubtedly slowed the public gaming sector's growth, with the absence of guidelines for the sector and, above all, the inability of concession holders to prepare financial plans of any type for their activities, especially in terms of investment.
The framework for tax reforms envisaged, in fact, a comprehensive overhaul of gaming. A number of important pointers 'towards the future' can be found in the document entitled 'Measures on gaming matters' sent to the Government by the ADM (the Customs and Monopolies Agency, the central controller of gaming in Italy) at the end of September. Although the contents of this document are not binding, analysis of the text identifies elements that may be used to rewrite the rules for the entire public gaming sector. Firstly, in the introduction to the document the ADM confirms that the system's failure to implement the framework for tax reforms represents a serious shortcoming, as well as the loss of an important opportunity that would have brought innovations to the entire sector, making it more efficient and productive. In fact, the ADM states that the enabling decrees referred to in Article 14 of the law dated 23 December 2013 (sic) would have allowed the pursuit of three important objectives:
1) the elimination of differences between the central and the territorial (regions and municipalities) governments, which have, according to the ADM document, "confused the overall regulatory framework, making the identification of true market opportunities highly uncertain"; to date, the regulations implemented by the territorial governments (regions and municipalities) conflict, placing restrictions on the opening and operation of betting shops and establishing bans and requirements, for example, to maintain a certain distance from so-called sensitive locations. Notably, even cemeteries are considered to be sensitive locations. Alongside this paradoxical situation, the rulings of various Regional Administrative Courts – appealed to by licence holders in order to uphold their rights granted by the State – have, by contrast, confirmed the legislative power of the regions on matters relating to public health. And, of course, it is considered necessary to protect public health against the risk of gambling addiction;
2) the creation, or rather, the 'recreation' of more reliable legal and market conditions in order to enable the holders of public gaming concessions to tolerate any additional demands on their resources that may be required;
3) the reformation of the regulatory framework put in place to tackle illegal gaming. In fact, despite the legalisation implemented by the 2015 Stability Law and the more intensive action against illegal activity taken in recent months by the Italian Authorities, the illegal market continues to thrive and therefore represents an added difficulty for legal operators.
Accepting the failure to implement the framework for tax reforms, the above three objectives and, in any case, summary guidelines for the survival of the entire gaming and betting sector, must still be implemented and achieved. Here, the ADM's planning document indicates three alternative approaches:
1) re-open the deadline for implementing the framework for tax reform;
2) formalise in a regulation the enabling decree referred to in Art. 14;
3) develop a limited package of regulations for inclusion in the draft Stability Law, with a view to recovering financial resources from the sector.
On the first point, there does not seem to be any room for 'reopening' a deadline that has long since passed. The second planning proposal, being the possible formalisation of the enabling decree as a primary regulation, appears to be more feasible. However much time is needed to approve a regulation of this size, involving the convergence of multiple interests, and considering the current difficulties faced in obtaining parliamentary approval for regulations, it is unlikely that this legislature would be able to transform the current draft into a regulation. At this point we must consider the third and final alternative, which does not in any case exclude the second, being inclusion in the 2016 Stability Law - remembering that the nature of this law excludes planning guidelines and only includes those associated with the accounts of the State – of certain indications about future calls for tenders (betting and bingo) that cannot be deferred any longer. For the survival of the system, it is obviously necessary to include instructions designed to resolve and/or attenuate the conflict between the State and the territorial governments, since continuation would utterly compromise both budgeting efforts and the investment made by gaming operators in Italy. The following indications on this, included in the ADM document, are worthy of support; they read "the regional and municipal regulations that effectively exclude legal public gaming should be" reviewed "commencing a political dialogue with ANCI and the Unified Conference, the scope of which may be decided with reference to the [...] points:
- gradual reduction in the number of amusement machines located in bars and similar locations (free access);
- obligation to certify premises (Betting shops, Bingo halls, VLT rooms)[...];
- obligation for legal gaming operators to attend periodic training sessions;
- make additional financial resources available to municipalities [...]."
Undoubtedly, these are all significant aspects. On the subject of periodic training, the writer believes that 'final mile' operators must be certified in order to lend certainty and solidity to the legal network, while representing a dignified and usable professional qualification. On the final point, the additional financial resources mentioned might include transfer to the municipalities of the fines imposed on illegal operators. In addition to assisting their finances, this would also help to reduce supply, and control the territory and criminal behaviour. This is a possible solution to an impasse that might otherwise wipe out the entire legal gaming sector.
Gaming and betting 2021: Law and practice
Gaming Law 2021: Trends and developments
Gaming Legislation: "Law and Practice"
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Reserve Bank of India suggests app to help visually impaired people identify rupee notes
Technology May 15, 2019
The visually impaired community in India is not able to access the new currency notes as they are inaccessible. This makes cash transactions challenging for around 80 lakh visually impaired people in the country.
The lack of identifiable features such as the dimensions and tactile marks, that can be felt and sensed by blind people through touch have made the new notes a huge headache.
The Reserve Bank of India says it is not feasible to completely remove the new notes from circulation, and has proposed to use technology to fix the problem. It has come forward with the idea of a mobile phone application that can be used to identify rupee notes.
While the move to find a solution, which comes after sustained pressure from disability rights groups, has been appreciated, technology may not offer the way forward says Mumbai-based lawyer Amar Jain.
I will say that it's one of the ways to solve the problem but it does not address the underlying problem of the physical currency being inaccessible by itself. I do understand the challenge of replacing a large volume of currency notes printed and there is cost involved in everything but at the same time we should take lessons from this and should ensure that at least the future designs of currency notes are accessible for blind people. I don't think to fix something like this with technology is a holistic approach. – Amar Jain, Lawyer
Technology companies interested in developing an app for currency identification have been asked to submit bids to the Reserve Bank of India.
The RBI has sent out a proposal in this regard that outlines the requirements from the app. The app needs to have features that are accessible and can be used easily by the blind people. Some of the features are:
– The app should be able to identify banknotes of Mahatma Gandhi Series and Mahatma Gandhi New series by capturing the image of the notes placed in front of mobile camera or scrolled across it.
– Should be able to identify the note within a duration of two seconds or less.
– Work in offline mode without Internet connection.
– Interface should be available with multi-lingual support or at least Hindi and English.
– Provide audio notifications.
– Users should be able to find the app in all the app stores using the voice option.
While the app may help some, what about those who do not have access to this technology? asks Vishal Kumar Jain.
Jain, who is a member of BGFI-Blind Graduates' Forum of India says, most people with visual disabilities in India do not have access to smartphones and have limited opportunities to learn using screen reading technology to operate a phone. "Also, the RBI doesn't seem to have conducted any structured user needs study before specifying the requirements in the tender", adds Jain. "Imagine the practicality of holding a white cane in one hand in a crowded noisy street, while using the other hand to hold the phone and point the camera accurately towards currency, without being able to see".
A better approach he says would be to have a small wearable device.
The Central Bank of India and the Centre will need to step up and make sure that such missteps do not occur again in the future and that whenever currency is designed, it is done with thorough consideration. This is true not just for currency but digital transactions, banks and ATMs too.
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Welcome to "The Adventures of Anna and Andy Hummingbird"
Me, Anna and Andy and the 6 year old!
I tell people I am just an average person. I grew up in Iowa City, Iowa and since then lived in Indiana, Michigan, Wisconsin and now I live in Las Vegas, Nevada. I love it here, NO SNOW!
I have training as an engraver, jeweler and sign maker. I have my own sign business and specialize in government mandated ADA signs, you know the ones with the little bumps you see in all public restrooms and suites. I enjoy my work and sometimes wish I had more time for writing.
I started writing the Anna and Andy series about seven years ago. I call the picture books "The Adventures of Anna and Andy Hummingbird." Anna and Andy are real and lived on my back patio for six years. I fell in love with them, and since my Grandchildren loved them too, I decided to write about them. I have a really great imagination, therefore it was not difficult to take some of the things I watched them doing and turn it into an adventure. "THE BEAST" in Book 2 is a perfect example. It is a 10 book series with, at this time, 1 thru 8 published. 9 and 10 will be completed in 2019. I have the the stories done, just need to finalize.
Many of the stories are true and Book 1 starts out with Anna and Andy being hatched on a beautiful Spring day.
My approach to writing was GO FOR IT! I knew I needed to make it easy to read, include colorful pictures and bold lettering. I turned myself into a 6 year old and jumped right in.
It is truly fun, and once I had my grammar fine tuned, (did use some editors) I went for it. I have since written three more children's picture books through Createspace (Amazon) and a couple of fiction books for adults and even though I know I am not perfect, I do my best. We all know not everyone is perfect, except maybe Stephen King! I hope you enjoy reading them to your children, that is why they were written.
The other books I have published outside of The Adventures of Anna and Andy Hummingbird will be featured in following pages.
If you are interested in the books you may e-mail me at annaandandyhummingbird@gmail.com You can also phone me at 702-364-5212, during the week I will answer with my business name but I almost always say "this is Linda."
I always have stock of my books and if you get them directly from me I can sign them for you!
Email or call me for prices. Hard cover or Soft cover and shipping costs.


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Why on Earth?
Secrets' Gate
VIDEOS?!
Recommendations!
LINKS/LIKES
Lilliputian Dictionary
The Author shares her worries with the Reader. Lemuel's first morning in his Prison-Temple; He discovers that he is being spied upon. He is making good progress learning Lilliputian, which he uses to beg for his Freedom. The first conditions are set out.
Redriff, Tuesday the 12th of September, 1702
Desolate Mary contemplating the future of her family.
Artist: Rembrandt van Rijn (1606-1669)
Lemuel (l) meets Flimnap (somewhere on the R)
Artist: Unknown
The little knight, holding the Report, dashing towards the Palace.
Lemuel is amazed at the Lilliputian's insolence.
Artist: Johann Sebastian Mueller (1715-1790)
Lilliputian lesson.
Artist: Thomas Morten (1836-1866)
WITH the fast approach of winter, my old fears are reviving. Can I provide for my children as befits the orphans of a ship-surgeon?
What am I thinking?
There is no evidence that Lemuel is dead!
Anyway, Johnny will have to start working soon. He is a strong lad, and big for a thirteen-year-old. But my Betty needs looking after. And what about the child in my belly..? Oh, I hope the curse is lifted, and that my baby will survive. I hope it will be a boy, not only because he will be able to provide for me when I am old, but also because he will be a constant reminder for me of my lost Lemuel, my lost Love.
But for now, all I have is the worries for my children, for my growing fatherless family. At least I have the memories of my nights with Lemuel and the stories he whispered in my ear at night, while hugging and caressing me.
These memories give me the power to live on and the hope against hope that our family will reunite in due course. Lemuel left us but three months ago and there was word that the 'Adventure' has reached the Cape of Good Hope on its way to Surat.
I believe with all my being that Lemuel is well.
He will come back to us in good time, having had a prosperous, eventless voyage -- unlike his last one, when he was cast ashore in Lilliput.
ON his first morning in his Prison-Temple, when Lemuel crept out, he was alarmed to see hundreds of Lilliputians surrounding the place. The Emperor gave specific orders that no Lilliputian was allowed to come near enough to Lemuel to be trampled on, so, from a safe distance, they all looked at him excitedly and expectantly.
Lemuel told me that he was so much hard pressed to give Water that he resolved to walk as far as his chains would allow him, round the Prison-Temple, where, he was relieved to see, no Lilliputian was to be seen.
The Volcano area seemed vacant enough, though more and more stalkers were rushing in that direction. But as soon as Lemuel opened his front flap, he was relieved to see how that act alone sufficed to scatter them all away.
Sighing with relief, Lemuel eased himself by giving Water to his heart's content, aiming carefully over the volcano, into the little river, which flowed into the ocean.
As soon as he turned around and came back to the entrance of his Prison-Temple, he noticed some little people running towards a couple of Hurgos, who were both sitting at a tiny table in front of his Prison-Temple, dressed in exquisite red attire.
Lemuel recognised one of them as the red-clad Lilliputian who addressed him from the stage, three days before, while he was still tied to the ground.
Some little people were talking excitedly to that Red man, who immediately wrote something with an almost invisible quill on a stamp size parchment. As Lemuel sat, leaning on the Temple's
wall, he saw the man rolling the parchment and rising from his chair. Bobbing confidently on his pair of very high heeled shoes, he approached Lemuel, bowed deeply and said:
"Clumglum Flimnap, dehul hekino. Hekina lang mar o clum slum Mildendo." (Meaning: "Minister Flimnap, at your service. Please be good to give this to my knight at the City Gate")
Of course, Lemuel did not understand a word of this at the time.
To his astonishment, Minister Flimnap then handed him the minuscule rolled parchment, and indicated to pass it on, waiving his hands to the left, in the direction of Mildendo, the metropolis.
When Lemuel got up and looked in that direction, he noticed a little knight, mounted on a little horse, standing at the gates of the city, looking expectantly at him. The knight at the gate probably had an amazingly good eye-sight, for he seemed to spot the parchment that Lemuel was carefully holding between his two fingers, and he began waiving frantically, gesticulating to Lemuel to hand the parchment over to him.
And indeed, when Lemuel bent over the fields that spread between his Prison-Temple and the City Gates, and handed the parchment to the Lilliputian knight, the parchment was snatched away from between his fingers, the knight tucked it under his arm and galloped on his little horse, with all his might, into town, in the direction of the Palace some yards away.
Lemuel followed the knight's slow progress for a while, and it suddenly dawned on him: these people were spying on him! They reported each and every move of his to the Emperor , and they had the audacity to use him as a messenger, to deliver those reports even faster!
Lemuel kept gazing at the knight, amazed at the Lilliputian's insolence, until he felt some irritating stabs at his right leg. Looking down, he saw a couple of Lilliputian soldiers, pointing spears at his ankle, tagging and retrieving as fast as they could. Minister Flimnap, standing at a safe distance too, was waiving and signalling to Lemuel to sit down again. Obediently, he did.
What else could he do?
The Minister thanked him officially and pointing at the other red-clad little man he said: "Loclum Reldresal, dehul hekino" (General Reldresal, at your service.)
While Minister Flimnap - clearly very relieved - was busy collecting his items and getting ready to leave, the General, who seemed to have no fear at all, came ever so near Lemuel, and pointing at himself, said: "Li Reldresal!" and pointing at Lemuel he asked very clearly: "Ina?"
Lemuel understood this quite well. In fact, in all the travel books he ever read, there have always been such dialogues of introductions. So he willingly replied: "Li Gulliver! Ina Reldresal!"
All the little people around were cheering in astonishment and Reldresal, obviously proud of himself, addressed the crowd:
"Gro Gulliver! Gro Quinbus Flestrin!" (He's Gulliver! He's a Man-Mountain!) And they all laughed good heartedly, including Gulliver, who did not want to appear any different than any of them.
And thus the Lilliputian lesson progressed, with Reldresal pointing at things around them and telling Gulliver their names.
Lemuel was a quick pupil and adamant to learn how to express his desire to get his Liberty. He gave many signs to that effect, pointing at his chained leg, bowing deeply and even waiving his hands as a bird, which did not make the impression he was hoping for.
As he waived his hands, the hem of his coat was swaying wildly and the wind blew Reldresal's papers away, as well as many a hat. The soldiers collected the papers promptly, people ran after their hats, and General Reldresal's answer was, as Lemuel could apprehend it, that Lemuel's freedom must be a work of time, not to be thought on without the advice of His Majesty's Council, and first he must "lumos kelmin pesso desmar lon emposo"; that is, "swear a peace with Him and His Kingdom."
However, General Reldresal made it clear that Lemuel should be used with all kindness; and, using simple words in Lilliputian, which Lemuel was swift to learn, combining many gestures and hand-signals, he managed to convey to Lemuel that in good time he would acquire, by his patience and discreet behaviour, the high opinion of His Royal Highness and His Subjects.
The first sign of such obedience, Lemuel guessed from General Reldresal's speech and gestures, was to let Certain Officers search Gulliver. This Lemuel could clearly fathom: they surely suspected that he might carry about him weapons, which would be dangerous things, judging by the bulk of so prodigious a person.
Lemuel said, part in his newly acquired Lilliputian, and part in signs, that he was ready to strip himself and turn up his pockets before any Officer of the Crown. He knew that his Condom is safely tucked away in his secret fob.
Please note that the FOOTNOTES might not show up on mobile devices. Go home and open your computer!


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NHS England looks to the future
As regular readers of our news page will know NHS England is preparing a major 10 year plan and better meeting the needs of people with Learning Disabilities and Autism is a key part of it all.
Make a date for the LDE Annual Conference!
Learning Disability England has announced that it is holding its Annual Conference in Manchester on Thursday January 24th 2019.
Vote KeyRing!
KeyRing (who provide supported living networks) have been shortlisted for some funding to help pay for financial support work in Nuneaton and Bedworth.
Transforming Care - Is it Working?
After the Winterbourne View scandal the government pledged to move people with disabilities out of unsuitable 'hospital' placements and into supported community living settings. This initiative was called 'Transforming Care'.
Advance Housing wins the double for HOLD!
We are delighted to announce that Advance Housing, who have supported more than 600 of our buyers over the past 20 years, won TWO prestigious National Housing Awards for HOLD last week!
Ready, aim, "dire"...DR UK blasts Universal Credit
Disability Rights UK has branded Universal Credit as "dire" and says that it is not fit for managed migration in its current form.
Sleep easier...
You may have seen that The Court of Appeal has made a ruling on Sleep In payments. The court found in favour of Mencap, so this means that the national minimum wage does not apply when a support worker is sleeping.
A List Not To Be Missed!
The Learning Disability and Autism Leaders' List 2018 is the UK's first national listing of people with learning disabilities and/or autism who are helping make things better for themselves and others.
Your Chance To Transform Transforming Care!
This is an urgent call to action as Norman Lamb MP has just secured a Westminster debate on the slow progress of Transforming Care.
T-Shirts Trump Trump!
In 'recognition' of the visit of Donald J Trump to the UK soon our colleagues at Learning Disability England have produced some t-shirts.


Sarnia Dentist Reviews - Read Our Testimonials Today!
At Dr. Karen Davis and Dr. John Milne Dentistry in Sarnia our standard of excellence and personalized care enable us to provide the dental services our patients deserve during every visit. If you are a new patient, please take a few moments to browse our submitted testimonials from patients who were happy to leave their Sarnia dentist reviews to see what kind of care you can expect at our office.
Thank you so much for the many hours of hard work, effort, and dedication that went into giving me a wonderful new smile! I just love it! The last few years have been a fascinating learning experience, which I have truly enjoyed. You have patiently answered all my questions, and I have always felt safe and comfortable working with you and Terri. Terri is the icing on the cake, always there to give support and encouragement, along with her contagious laughter. You make a great team, and your friendly banter has made my day many times.
How did my new smile begin? I planned on having old fillings replaced and ended up going on a journey I never expected to take, but one that was worth every smile of the way!
Thanks again, Dr. Milne, for everything. You gave me something I will always treasure – my wonderful new smile!
Having been a patient of yours for several years, I just wanted to let you know how much I appreciate you and your staff. You're all very courteous, professional people, who genuinely care about your patients. From the warm smiles to the great sense of humour, you are a dedicated group who specialize in making me feel welcome and extremely comfortable. I actually look forward to my dental appointments, not only because your chairs are so comfortable, but because it is always a gentle, pain-free, and pleasant experience. You always have the most state-of-the-art equipment and provide the most stress-free visits I have ever experienced. I am grateful to have found a dentist who takes the time to discuss my treatment and make sure all my questions and concerns are addressed in a patient and caring manner. I highly recommend you to all of my friends, family, and co-workers. I feel truly blessed to be a patient of yours!
For many, many years, I have looked at people who have pretty smiles and have always thought that I could never have one. My teeth were just one of my many imperfections I had and contributed to my lack of self-esteem. Then, I was given the opportunity to change my smile. My teeth were going to have a dramatic makeover, and I had a second chance to get life right. The procedure at first seemed quite intense, with a lot of preparation going in, which in the end only led to perfection. I cannot thank Dr. John, Terri, and the rest of the team for their kindness and professional care I received. Thank you again for giving me this opportunity.
I truly appreciate all you've done for me; I've referred you to all of my friends and family! Only good people are worthy of your talents!
I have since become a new patient of Dr. Karen Davis. I was shocked at how thorough and efficient she and the team were. My past experiences have been less than favourable; I was very nervous, and they all put me at ease. Thank you, Dr. Davis, for all your time and patience!
Just a quick note of appreciation! The New Patient Exam… I thought I was in a different city than in Sarnia … it felt like a resort. The customer service made me "almost" look forward to my next visit, which was the root canal. The actual root canal visit exceeded those feelings, and it was actually pleasurable. I have never had such a good dental experience and have since told many that "this is the place to go!" I was golfing that same night and have had only very minor subsequent discomfort. The actual surgery was nothing more than keeping my mouth open for a bit, and I am good at that! That evening, the dentist called me to see how I was doing, which I have never experienced! Thank you so much for making the visit so good, and the only place I will continue for care!


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by Aidan Gibbons
WWE Planning Gimmick Change For The Revival
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Home » "I went to Africa," Wellsville's Harrison Reagan makes an epic speech on his recent trip
"I went to Africa," Wellsville's Harrison Reagan makes an epic speech on his recent trip
Reagan and his mother, Shaye, traveled to Kenya to support Rehema House
Harrison is in the fifth grade at Immaculate Conception School in Wellsville
By Andrew Harris, pictures by Shaye Reagan
Traveling to another continent is something most people never do. Fifth grader Harrison Regan is officially a transcontinental traveler after a journey to Kenya on a humanitarian mission.
Harrison, and his travel companion, mother Shaye Reagan have recently returned from a quick, eight day trip to Nairobi, Kenya. The duo had a primary mission to serve the orphanage at Rehema Home, where about 100 children call home.
Before leaving, the duo was asked to bring lots of shoes, socks and underwear. It is important to the missionaries of Rehema Home to make sure each child is outfitted with shoes, but the reality is that many children in Kenya who are orphaned or live in poverty are without these items. With generous financial gifts and donations from within the community they were able to take 255 pair of shoes of all sizes, along with nearly 75 pounds of socks and underwear. Each child – toddler up through age 18 – we able to hand-select shoes that perfectly fit them and their personalities.
Reagan told the crowd gathered in the cafeteria of his Immaculate Conception School that the journey took three plane rides and a full twenty-four hours of travel. The fifth grader started the talk by saying to the audience, "I don't know anyone here would pass up a trip to another continent!!"
Did you know ALCO is now serving Steuben County ? Tap to learn more…
Riding motorcycles, standing on the equator, going on a wild safari and petting a rhino! These are just some of the amazing things that Harrison experienced in Africa. Harrison's talk to fellow classmates and his teachers had a very serious theme about something that we all need: Water.
*Before we get into the serious part of the speech…. Harrison is a gifted public speaker, mixing prepared remarks with off-the-cuff commentary. Reagan, as if he has been to college and back, was able to present to the crowd in a very effective and entertaining way. So impressive for a ten year old.
Water, something that Wellsville takes for granted with a river and a modern water treatment facility, was a major theme of Harrison's speech. In Kenya, water can be dangerous and those who have not been acclimated to the flora must take special care, according to Harrison. Visitors like the Reagan's had to be very careful with water, using purified water only. The locals are able to drink some well water and rainwater because they have acclimated to the native bacteria.*
To obtain clean water for a household, many walk long distances barefoot and return with large water vessels carried on top of thier heads, called "jerry cans." That iconic African imagery that we have all seen, is a real daily part of life for Kenyans.
Harrison ended his remarks about the realities of clean water in Africa by previewing an initiative that his school, Immaculate Conception School in Wellsville is about to undertake. Harrison's trip has inspired the school to take action and help others on the other side of the planet. A rare case where the student is teaching the school!
After wrapping up his prepared marks with the skill of a future President, Harrison opened up the talk to questions from the audience. Many hands went in the air when asked, with some great questions.
QUESTION: What is different about the kids in Kenya you stayed with?
Harrison: Nothing! They are just like us, except they don't have parents, which is bad."
QUESTION: What are the kids houses like?
Harrison: Well they are not grass shacks!! Most are made of concrete and clay, they are very pretty
QUESTION: How do African's eat ?
Harrison: Just like you mostly, many meals are served on bread. Kinda of a squishy pancake that use to hold the food and eat.
QUESTION: What would happen if they stepped on an African porcupine quill ?
Harrison: They would get poked !!
QUESTION: How long is their school day?
Harrison: Long. They start early in the morning and don't get home until about 5pm. They go to school all year long and even on the weekends sometimes.
QUESTION: How many kids live in the orphanage?
Harrison: About 100.
QUESTION: Do they have cell phones and devices?
Harrison: Yes they do but they play lots of sports, play music, and have a nice playground.
The speech ended with a loud round of applause which Harrison appreciated. Clearly this young man has learned alot from his trip. His school mates were not only impressed but curious about international travel and doing mission work. My bet is that this will not be last intercontinental journey for Harrison and his enthusiasm may even inspire is classmates and freinds!
*There is some truth to the fact that locals can have some resistance toward cholera, typhoid, and other water-bourne illnesses. But many kids have gotten sick from drinking this contaminated water. Kids at Rehema Home do have access to medical care, though the government infrastructure doesn't provide affordable care for at-risk populations. Access to healthcare is costly for Rehema Home and is funded through donations to the organization. For many who are already immunocompromised, exposure to contaminated water can bring about severe illness and even death.
Learn more about Rehema Home: https://www.rehemahome.org/
Hornell Public Library Presents Artist of the Month: Hope Zaccagni
Meet the artist: Shawn Forshee, view slideshow
Fruitcake Presentation will mark the end of 2022 Steuben County Legislature
Bob Confer Column: A national crisis in rare earth elements


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

As the most massive bound systems known, galaxy clusters provide an important link in understanding the composition and growth of structure in the Universe.  Clusters follow a variety of observational scalings of mass with temperature, luminosity, or cluster counts, and these scalings are sensitive to cosmological parameters including the matter density parameter $\Omega_{\rm m}$, the cosmological constant density parameter $\Omega_\Lambda$, the dark energy equation-of-state parameter $w$, and the normalization of the matter power spectrum $\sigma_8$ (e.g., \citealt{HA01.2,BA02.2,LE02.1,SC03.2,AL04.2,VI09.1}).  Such constraints from galaxy clusters complement the constraints on cosmological parameters from Type Ia supernovae and cosmic microwave background observations.

However, useful galaxy cluster constraints on cosmological parameters
depend primarily on accurate determinations of cluster masses.  Observationally,
cluster masses are typically measured in one of three ways.

A long-established method for determining cluster masses employs the
virial theorem and the measurement of
velocities of the galaxies that constitute the cluster.  Based on the
three assumptions that the cluster is in virial equilibrium, the galaxy distribution efficiently traces
the cluster mass distribution, and the velocity dispersions
$\sigma$ of the galaxies are isotropic, the cluster mass contained within a radius
$r$ is estimated $M \sim \sigma^2 r/G$.  However, these mass estimates
may be biased as a result of galaxy velocity anisotropies or if
the galaxy distribution does not follow the total mass
distribution (e.g., \citealt{BA82.1}).

A second method uses cluster X-ray emission as a tracer of cluster masses.
The hot intracluster gas, which is the dominant baryonic component of a cluster and is typically twice the mass of the total mass of the galaxies
in a cluster, emits X-rays via bremsstrahlung radiation and atomic
line emission.  With the temperature $T$ and radial density
$\rho(r)$ profiles determined
from X-ray spectra and surface brightness distributions, the cluster
mass is given by $M \sim r^2/\rho(r) \; d(-\rho T)/ dr$.  This method assumes
that the intracluster gas is spherically distributed and is in hydrostatic
equilibrium \citep{EV96.1}.  However, these assumptions may be
incorrect. If the gas distribution is not spherical, X-ray mass estimates will be biased by projection effects.  Many galaxy clusters are also not in hydrostatic equilibrium, in particular dynamically unrelaxed clusters that are
undergoing mergers.  There is evidence that the bias of hydrostatic equilibrium mass is linked to the dynamical state of the galaxy cluster (e.g., \citealt{AN09.1,ZH09.1}). In
addition, the hot gas of galaxy clusters with buoyant bubbles near their cores might indicate a departure from hydrostatic equilibrium (e.g.,
\citealt{CH01.1}).

The most direct estimates of cluster masses employ gravitational lensing
distortions of background galaxies.  This technique is free of
assumptions about the dynamical state of the cluster, which enables it in
principle to yield more consistent mass estimates, though it is also sensitive to projection effects.  More accurate
cluster mass
estimates can in turn provide tighter constraints on cosmological parameters, and therefore it is of key importance to reduce the errors in cluster mass estimates.

For example, the primary source of error in cluster-based determinations of
$\sigma_8$ is the error in the mass-temperature relation for relaxed
clusters (e.g., \citealt{PI03.1,HE04.2,VO05.1}).  Recent studies show that an X-ray independent mass approach such as gravitational lensing provides a unique tool to calibrate the mass - temperature relation (e.g., \citealt{SM05.1, MA08.1, ZH08.1}).
Here, we use strong gravitational lensing mass measurements of a sample of eight strong
lensing clusters at $0.3 < z
< 0.8$ to accurately measure the galaxy cluster mass-temperature
relation.  We also include the effects of cluster concentrations in an
effort to further reduce the scatter in the cluster mass-temperature
relation, which would ultimately enable tighter constraints on
$\sigma_8$.

In addition to the correlations that exist between cluster properties,
some observational properties of brightest cluster galaxies (BCGs) also
scale with
properties of the host clusters.  Whereas scalings between cluster
properties are
sensitive to
cosmological parameters, scalings between BCGs and their host clusters
provide constraints on BCG
formation and the evolution of clusters.

BCGs are a unique population: they are the most massive and luminous galaxies in the Universe.  They are typically located near the centers of clusters, which suggests that a BCG's formation history is intricately linked to the formation of the cluster itself. However, the formation of BCGs is still poorly understood.

BCGs may form after their host clusters assemble in one of two ways.  First, a
BCG may be the first galaxy to be dragged in by dynamical friction to the center of the dark
matter halo destined to become a cluster, where it then grows through galactic cannibalism by
merging with subsequent galaxies that fall to the center (e.g.,
\citealt{OS75.1,HA78.1}).  However, this scenario typically requires more than a
Hubble time to form a BCG because much of the mass of the infalling galaxy is tidally
stripped, which reduces the dynamical friction effect and slows the
infall \citep{ME85.1}.

BCG formation may also occur after cluster formation if the host cluster's
central cooling flow forms stars at the cluster center and those stars
build the BCG \citep{CO77.1}. There are several instances of ongoing or recent star formation in BCGs that occupy cooling-flow clusters (e.g., \citealt{CA98.1,CR99.1, HI05.1,MC06.1}), but it is unclear whether the star formation is fueled by the cooling flows or by cold gas brought in through recent galaxy mergers \citep{BI08.2}.

In another scenario, BCGs might form in concert with their host clusters.
A BCG may begin with several galaxies merging together in a group to
form a large galaxy, and then when groups merge as hierarchical
structure formation continues, this large galaxy eventually becomes a
BCG in a massive cluster (e.g., \citealt{ME85.1, DU98.1, BO06.1}).

Here, we examine the correlation between BCG luminosity and cluster
mass in eight strong
lensing clusters at $0.3 < z
<0.8$.  This will enable constraints not only on BCG and cluster formation in general,
but also on how the BCGs in strong lensing clusters may have formed
and evolved differently than BCGs in the general cluster population.

The rest of this paper is organized as follows.
In Section~\ref{sample} we describe the selection of our cluster sample, and Section~\ref{properties} gives the masses, dynamical states, and X-ray temperatures for these clusters.  In Section~\ref{mtrelation} we find the $M-T$ relation for the relaxed clusters in our sample and show how the inclusion of cluster concentrations both significantly reduces the scatter in the $M-T$ relation and lifts the restriction on cluster dynamical state.  In Section~\ref{bcgprop} we identify the BCGs in our sample and measure their luminosities. We use these luminosities in Section~\ref{lm} to measure the correlation between BCG luminosity and cluster mass, and we find preliminary evidence that strong lensing clusters may have more active merging histories than the general cluster population.  Section~\ref{conclude} presents our conclusions.
Throughout this paper, we adopt a spatially flat cosmological model
dominated by cold dark matter and a cosmological constant ($\Omega_{\rm m}=0.3$,
$\Omega_\Lambda=0.7$, $h=0.7$).

\section{Sample Selection}
\label{sample}

We base our sample on 10 well-known strong lensing clusters
analyzed in \cite{CO06.1}.  All 10 clusters have {\it Hubble Space
  Telescope} ({\it HST}) imaging, which make possible the mass determinations
and photometry measurements central to this paper.  However,
there are no published arc redshifts for two of the clusters, Cl~0016$+$1609
and Cl~0054$-$27, which limits the strong lensing determination of their
cluster masses to the unknown factor $D_{\rm s}/D_{\rm ls}$, the ratio of the
angular diameter distances to the source and between the lens and
source.  Consequently we remove these two clusters, and our sample consists of the
remaining eight clusters at $0.3 < z < 0.8$: ClG~2244$-$02, Abell~370, 3C~220.1,
MS~2137.3$-$2353, MS~0451.6$-$0305, MS~1137.5$+$6625, Cl~0939$+$4713,
and ZwCl~0024$+$1652.

\section{Cluster Properties}
\label{properties}

Strong correlations are found between cluster observables, and the resultant scaling relations clearly encapsulate key information about cosmological parameters and the assembly history of clusters.  Cluster masses are a component of many cluster scaling relations, and we measure strong lensing masses for our sample of clusters and
compare these to mass estimates from the distributions
of cluster X-ray gas.  Based on
these comparisons and other observable properties of the cluster, we
determine the dynamical state of each cluster as relaxed or
unrelaxed.  We also present cluster X-ray temperatures, which are another component of cluster scaling relations.

\subsection{Cluster Strong Lensing Mass Determination}
\label{mass}

We model each cluster mass distribution with an elliptical Navarro-Frenk-White
(NFW; \citealt{NA96.1, NA97.1}) dark
matter halo centered on the BCG, using the best-fit NFW parameters found by \cite{CO06.1}.
Strong lensing
arcs with measured redshifts observed in a cluster constrain its mass distribution, and
\cite{CO06.1} use the arcs to characterize best-fit NFW ellipsoids
to each cluster.  With the NFW dark matter
halos completely defined in this way, we can determine any
cluster radius
$r_{\Delta}$ as the radius at which the density of the halo is $\Delta$ times
the critical density at the cluster redshift.

Lack of information about the clusters' three-dimensional shapes
prevents us from calculating their elliptical masses, but
instead we determine the equivalent mass of a spherical NFW halo.
With the \cite{CO06.1} best-fit scale convergence $\kappa_\mathrm{s}$
and scale radius $r_\mathrm{s}$, we estimate the cluster mass within radius $r_\Delta$ as

\begin{equation}
 M_\Delta=4\pi\Sigma_\mathrm{crit}\kappa_\mathrm{s}r_\mathrm{s}^2\,
  \left[\ln(1+x)-\frac{x}{1+x}\right]\;,
\end{equation}
where $x \equiv r_\Delta/r_\mathrm{s}$ and $\Sigma_\mathrm{crit}$ is
the critical surface mass density, defined as
\begin{equation}
\Sigma_\mathrm{crit} \equiv \frac{c^2} {4 \pi G} \frac{D_{\rm s}} {D_{\rm l}
  D_{\rm ls}} \; ,
\end{equation}
which depends on the angular diameter distances $D_{\rm l,s,ls}$ from the
observer to the lens, to the source, and from the lens to the source,
respectively.

We estimate the errors in mass by propagating the errors in the
best-fit NFW parameters.  As detailed in \cite{CO06.1} these errors
are quite small but are realistic, because the reproduced lensed
image is sensitive to slight variations in a parameter's value.
However, we note that these errors are relevant only to the choice of
lens model and data and do not represent a global systematic uncertainty.

We use the method described here to measure the lensing cluster masses in Table~\ref{tbl:mass},
as well as the cluster masses $M_{200}$ and $M_{2500}$ in Table~\ref{tbl:props}.

\begin{deluxetable*}{lllllllll}
\tablewidth{0pt}
\tablecolumns{9}
\tablecaption{Comparisons between strong lensing and X-ray cluster mass
  estimates.}
\tablehead{
\colhead{Cluster} &
\colhead{$\Delta$} &
\colhead{$r$} &
\colhead{$M_{\mathrm{lens}}(\leq r)$} &
\colhead{$M_{\mathrm{X-ray}}(\leq r)$} &
\colhead{$M_{\mathrm{lens}}(\leq r)/$} &
\colhead{Reduced} &
\colhead{Dynamical} &
\colhead{Reference} \\ & &
\colhead{$(h_{70}^{-1}$ Mpc)} &
\colhead{$(10^{14} \, h_{70}^{-1} \, M_\odot)$} &
\colhead{$(10^{14} \, h_{70}^{-1} \, M_\odot)$} &
\colhead{$M_{\mathrm{X-ray}}(\leq r)$} &
\colhead{$\chi^2$} &
\colhead{State} &
}
\startdata
ClG~2244$-$02 & 500$\, \Omega^{0.427}$ & $0.83^{+0.26}_{-0.20}$ &
$2.85^{+1.25}_{-0.99}$ &
$1.50^{+1.07}_{-0.63}$ & $1.90^{+2.81}_{-1.18}$ & 0.91 & Relaxed & 1 \\
& 18$\pi^2 \, \Omega^{0.427}$ & $1.31^{+0.42}_{-0.31}$ &
$4.22^{+1.63}_{-1.27}$ & $2.37^{+1.73}_{-0.99}$ &
$1.78^{+2.46}_{-1.06}$ &
0.86 & & 1 \\
Abell~370 & 500$\, \Omega^{0.427}$ & $1.15^{+0.28}_{-0.20}$ &
$6.45^{+2.04}_{-1.52}$ & $4.19^{+2.06}_{-1.30}$ &
$1.54^{+1.40}_{-0.75}$ & 0.85 & Unrelaxed & 1 \\
& 18$\pi^2 \, \Omega^{0.427}$ & $1.81^{+0.44}_{-0.32}$ &
$9.25^{+2.50}_{-1.92}$ &
$6.73^{+3.57}_{-2.16}$ & $1.37^{+1.20}_{-0.66}$  & 0.49 & & 1 \\
3C~220.1 & 500$\, \Omega^{0.427}$ & $1.17^{+0.45}_{-0.25}$ &
$3.22^{+1.37}_{-0.80}$ & $5.80^{+5.25}_{-2.19}$ &
$0.56^{+0.72}_{-0.34}$ & 0.44 & Relaxed & 1 \\
& 18$\pi^2 \, \Omega^{0.427}$ & $1.74^{+0.67}_{-0.37}$ &
$4.25^{+1.56}_{-0.92}$ &
$8.64^{+7.85}_{-3.27}$ & $0.49^{+0.59}_{-0.29}$ & 0.59 & &1 \\
MS~2137.3$-$2353 & 2500 & $0.46^{+0.02}_{-0.03}$ &
$1.62^{+0.18}_{-0.19}$ & $1.89^{+0.25}_{-0.31}$ &
$0.86^{+0.28}_{-0.19}$ & 0.65 &
Relaxed & 2 \\
& 500$\, \Omega^{0.427}$ & $1.07^{+0.10}_{-0.06}$ &
$2.73^{+0.34}_{-0.30}$ & $3.16^{+0.60}_{-0.36}$ &
$0.86^{+0.23}_{-0.22}$ & 0.57 & & 1 \\
& 18$\pi^2 \, \Omega^{0.427}$ & $1.69^{+0.15}_{-0.10}$ &
$3.40^{+0.40}_{-0.37}$ & $4.99^{+0.95}_{-0.57}$ &
$0.68^{+0.18}_{-0.17}$ & 3.5 & & 1 \\
MS~0451.6$-$0305 & 500$\, \Omega^{0.427}$ & $1.38^{+0.25}_{-0.20}$ &
$13.4^{+3.1}_{-2.6}$ & $8.90^{+3.44}_{-2.31}$
& $1.50^{+1.00}_{-0.63}$ & 1.2 & Unrelaxed & 1 \\
& 18$\pi^2 \, \Omega^{0.427}$ & $2.09^{+0.38}_{-0.30}$ &
$18.3^{+3.7}_{-3.2}$ & $13.6^{+5.4}_{-3.6}$ &
$1.34^{+0.86}_{-0.55}$ & 0.68 & & 1 \\
MS~1137.5$+$6625 & 500$\, \Omega^{0.427}$ & $1.41^{+1.26}_{-0.45}$ &
$6.80^{+7.22}_{-2.64}$ & $12.5^{+32.0}_{-6.7}$
& $0.54^{+1.87}_{-0.45}$ & 0.082 & Relaxed & 1 \\
& 18$\pi^2 \, \Omega^{0.427}$ & $2.06^{+1.84}_{-0.66}$ &
$9.10^{+8.34}_{-3.08}$ & $18.2^{+46.9}_{-9.8}$
& $0.50^{+1.58}_{-0.41}$ & 0.099 & & 1 \\
Cl~0939$+$4713 & & $0.36$ & $0.38 \pm
0.05$ & $0.72 \pm 0.21$ & $0.53^{+0.31}_{-0.17}$ & 2.5 & Unrelaxed & 3 \\
& & $0.71$ & $0.69 \pm 0.08$ & $2.13 \pm 0.50$ &
$0.32^{+0.15}_{-0.09}$ & 8.1 & & 3 \\
ZwCl~0024$+$1652 & 500$\, \Omega^{0.427}$ & $0.94^{+0.39}_{-0.21}$ &
$2.02^{+0.97}_{-0.54}$ & $2.31^{+2.34}_{-0.91}$ &
$0.87^{+1.26}_{-0.56}$ & 0.027 & Unrelaxed & 1 \\
& 18$\pi^2 \, \Omega^{0.427}$ & $1.45^{+0.61}_{-0.32}$ &
$2.77^{+1.15}_{-0.64}$ & $3.59^{+3.63}_{-1.41}$ &
$0.77^{+1.03}_{-0.48}$ & 0.094 & & 1 \\
\enddata

\tablerefs{(1) \cite{OT04.2}; (2) \cite{AL01.2}; (3) \cite{DE03.1}.}

\label{tbl:mass}
\end{deluxetable*}

\subsection{Dynamical State of Clusters: \\ Relaxed vs. Unrelaxed}
\label{relax}

Since one of our aims is to measure the mass-temperature relation for
relaxed lensing clusters, we must determine which of the eight clusters in our sample
are dynamically relaxed.
X-ray cluster mass estimates are based on the
assumption that the cluster is in hydrostatic equilibrium, and if a
cluster is relaxed it is also in hydrostatic equilibrium.  Therefore,
X-ray mass measurements for relaxed clusters should be accurate and
consistent with lensing mass measurements.

We use X-ray mass estimates from the literature, where the X-ray masses are measured for each cluster at two or three different radii.  For each cluster, Table~\ref{tbl:mass} gives the lensing mass and X-ray
mass measured
within the two or three different cluster radii.  Table~\ref{tbl:mass} also shows the lensing mass to X-ray mass ratio and the
reduced $\chi^2$ of the comparison of lensing and X-ray masses.  For six
clusters, at all radii at which masses were measured, the ratio of lensing mass to X-ray mass is consistent
with unity and the reduced $\chi^2$ is $\lesssim 1$, suggesting
that these six clusters could be relaxed.  Additional observational evidence in \S~\ref{relaxed} and \S~\ref{unrelaxed} shows that four of these six
clusters are relaxed, while the
remaining two clusters are unrelaxed.

For at least one of the radii considered, the two clusters MS~2137$-$23 and Cl~0939$+$4713 each exhibit lensing to X-ray mass ratios that are
inconsistent with unity and reduced $\chi^2$ that are greater than
unity, which is evidence that the clusters are unrelaxed.  We measure
masses for MS~2137$-$23 within three different radii, and within one
of these radii the mass ratio is
inconsistent with unity and the reduced $\chi^2$ is greater than
unity.  However there
is opposing evidence, given in \S~\ref{relaxed}, that characterizes MS~2137$-$23 as a
relaxed cluster. For Cl~0939$+$4713, the mass ratios measured at both
radii considered are inconsistent with unity and both reduced $\chi^2$ are much
greater than unity, suggesting Cl~0939$+$4713 may be an
unrelaxed cluster.  In \S~\ref{unrelaxed} we present more evidence in support of this
conclusion.

Additional information about the dynamical state of a cluster can be found in its X-ray emission map.  For example, the position of the BCG relative to the peak in the cluster's X-ray profile may be evidence of a cluster's dynamical state: if the two are coincident the cluster is likely relaxed, otherwise it is likely unrelaxed.  The centroid shift is one means of quantifying this positional difference (e.g., \citealt{MO93.1, JE08.1}).  Additionally, a smooth distribution of X-ray gas indicates the cluster is likely in a relaxed state.  However, if the X-ray gas is distributed irregularly or shows evidence of shocks or substructure, the cluster is likely unrelaxed and undergoing a merger.
Below we examine evidence for the dynamical state of each cluster
individually and label
each cluster as relaxed or unrelaxed (these labels are also given in
Table~\ref{tbl:mass}).  We first discuss the four relaxed clusters, then the
four unrelaxed clusters.

\subsubsection{Relaxed Clusters}
\label{relaxed}

\begin{itemize}

\item \textbf{Cl~2244$-$02}:
We find that X-ray and lensing masses for Cl~2244$-$02 are consistent
(Table~\ref{tbl:mass}) and \cite{OT98.1} also find
consistent X-ray and lensing masses, suggesting that hydrostatic
equilibrium is a valid assumption for Cl~2244$-$02 and that it is a relaxed
cluster.

\item \textbf{3C~220.1}: The radial profile of X-ray emission from
  3C~220.1 shows no sign of
irregularity and the profile is well-fit by a model assuming
hydrostatic equilibrium, which suggest that 3C~220.1 is a relaxed
cluster \citep{WO01.1}.

\item \textbf{MS~2137$-$23}: The X-ray and strong lensing masses of MS~2137$-$23 are in good agreement \citep{AL98.1}, indicating that it is in a relaxed state.  Many relaxed clusters also have cooling flows, such as the massive cooling flow in MS~2137$-$23
\citep{AL98.1, WU00.1}.

\item \textbf{MS~1137$+$66}: The cluster MS~1137$+$66 not only has consistent X-ray and weak lensing
masses (Table~\ref{tbl:mass}), but also has a small centroid shift \citep{MA08.2} and may host a moderate cooling flow \citep{DO99.1}.  In
addition, Sunyaev Zel'dovich observations of the cluster show no
obvious substructure \citep{CO02.1}.  These properites connote that
MS~1137$+$66 is a relaxed cluster.

\begin{deluxetable*}{llllll}
\tablewidth{0pt}
\tablecolumns{6}
\tablecaption{Cluster lensing masses and
  X-ray temperatures.}
\tablehead{
\colhead{Cluster} &
\colhead{$z$} &
\colhead{$M_{200}$} &
\colhead{$M_{2500}$} &
\colhead{$k T$} &
\colhead{Reference} \\ &&
\colhead{$(10^{14} \, h_{70}^{-1} \, M_\odot)$} &
\colhead{$(10^{14} \, h_{70}^{-1} \, M_\odot)$} &
\colhead{(keV)}
}
\startdata
ClG~2244$-$02 & 0.33 & $4.5 \pm 0.9$ & $1.3 \pm 0.2$ & $4.85^{+1.25}_{-0.96}$ & 1 \\
Abell~370 & 0.375 & $9.0 \pm 1.0$ & $2.9 \pm 0.3$ & $7.20^{+0.75}_{-0.77}$ & 1 \\
3C~220.1 & 0.62 & $3.1 \pm 0.3$ & $0.91 \pm 0.10$ & $5.6^{+1.5}_{-1.1}$ & 2 \\
MS~2137.3$-$2353 & 0.313 & $2.9 \pm 0.4$ & $1.5 \pm 0.2$ & $4.57^{+0.41}_{-0.35}$ & 1 \\
MS~0451.6$-$0305 & 0.55 & $18 \pm 2$ & $6.3 \pm 0.7$ &
$8.62^{+1.54}_{-1.21}$ & 1 \\
MS~1137.5$+$6625 & 0.783 & $6.5 \pm 0.7$ & $1.5 \pm 0.2$ & $6.70^{+1.84}_{-1.46}$ & 1 \\
Cl~0939$+$4713 & 0.41 & $0.71 \pm 0.11$ & $0.21 \pm 0.03$ & $7.6^{+2.8}_{-1.6}$ & 3 \\
ZwCl~0024$+$1652 & 0.395 & $2.3 \pm 0.2$ & $0.69 \pm 0.07$ & $5.17^{+1.95}_{-1.34}$
& 1 \\
\enddata

\tablerefs{(1) \cite{HO01.1}; (2) \cite{OT00.1}; (3) \cite{SC98.3}.}

\label{tbl:props}
\end{deluxetable*}

\subsubsection{Unrelaxed Clusters}
\label{unrelaxed}

\item \textbf{Abell~370}: Abell~370 hosts two cD galaxies, and there are X-ray peaks centered on each cD
\citep{ME94.1}.  The two
cD galaxies are moving relative to each other at 1000 km s$^{-1}$,
signaling that Abell~370 is an unrelaxed cluster undergoing a merger
\citep{KN93.1}.

\item \textbf{Cl~0939$+$4713}: X-ray observations of Cl~0939$+$4713 show evidence for substructure
\citep{SC96.3}, and the disagreement between lensing and X-ray masses
shown in Table~\ref{tbl:mass} further suggests that Cl~0939$+$4713 is not in hydrostatic
equilibrium.  These observations indicate Cl~0939$+$4713 is an unrelaxed cluster.

\item \textbf{Cl~0024$+$17}: The two dark matter clumps near the center of Cl~0024$+$17 are separated in redshift, implying that it is a merging cluster \citep{NA09.1}. There is additional evidence for substructure in Cl~0024$+$17 in its mass
models, which require substructure to produce a good fit to the cluster's
lensing arcs \citep{BR00.1}.  The redshifts of the member galaxies are
distributed bimodally, fortifying the evidence that
Cl~0024$+$17 may have undergone a merger with another cluster
\citep{CZ02.1}.  The evidence implies that Cl~0024$+$17 is an unrelaxed cluster.

\item \textbf{MS~0451.6$-$0305}: The distribution of mass within the central 1$^\prime$ of MS~0451.6$-$0305 is not smooth, and the centroid shift indicates the BCG is not located at the X-ray peak \citep{BO04.2, MA08.2}.  These observations suggest that MS~0451.6$-$0305 is unrelaxed.

\end{itemize}

\subsection{Cluster X-ray Temperatures}
\label{temp}

The temperature of the intracluster medium is commonly measured
using its X-ray emission in one of several ways:
through fits to the cluster's observed X-ray spectrum (yielding the spectroscopic temperature $T_{\rm s}$), through
weighting by the mass of the gas element (yielding the mass-weighted temperature
$T_{\rm m}$), or through weighting by the emissivity of the gas
element (yielding the emission-weighted temperature $T_{\rm em}$).  However, the spectroscopic temperature $T_{\rm s}$
is systematically lower than the mass-weighted temperature $T_{\rm m}$ and
the emission-weighted temperature $T_{\rm em}$
\citep{MA01.2, MA04.1}, so an accurate temperature comparison across different clusters requires consistent temperature measurements.

To ensure that the cluster temperatures we use for our sample are as
consistent as possible, we use the mean cluster temperatures derived
from the single-temperature model fits of {\it ASCA} data in \cite{HO01.1}.  This large,
homogeneous catalog of spectroscopic cluster temperatures
includes six of our clusters, and for the
remaining two clusters, 3C~220.1 and Cl~0939$+$4713, we remain as
consistent as possible by using
spectroscopic temperatures from single-temperature
fits.   Table~\ref{tbl:props} gives the cluster
temperatures and the corresponding references. We note that none
of the temperatures we use apply corrections for
cool cores at the cluster centers.

Some clusters in our sample also have temperature measurements from {\it Chandra} and {\it XMM-Newton} data.  Specifically, 3C~220.1 has a {\it Chandra} temperature of $8.5^{+3.7}_{-2.3}$ keV within 10 -- 45$^{\prime\prime}$ \citep{WO01.1}; MS~0451.6$-$0305 has a {\it Chandra} temperature of $6.7^{+0.6}_{-0.5}$ keV within $r_{500}$ \citep{MA08.2}; MS~1137.5$+$6625 has a {\it Chandra} temperature of $5.8^{+0.7}_{-0.6}$ keV within $r_{500}$ \citep{MA08.2}; and Cl~0024$+$17 has an average {\it Chandra} temperature of $4.47^{+0.83}_{-0.54}$ keV  \citep{OT04.1} and an {\it XMM-Newton} temperature of $3.52 \pm 0.17$ keV within 3$^\prime$ \citep{ZH05.2}.  Use of {\it Chandra} or {\it XMM-Newton} temperatures could change the results of the mass-temperature relation.  However, because {\it Chandra} and {\it XMM-Newton} temperatures have been measured for only a subset of our sample, and because these temperatures are measured within inconsistent cluster radii, we do not use {\it Chandra} and {\it XMM-Newton} measurements in our determination of the cluster mass-temperature relation below.

\section{The Mass-Temperature Relation}
\label{mtrelation}
Theoretical arguments suggest a correlation between cluster mass and
X-ray temperature for relaxed clusters, which provides the link
between the gas in a cluster and its mass.  Here we determine the
cluster mass-temperature relation for relaxed {\it strong lensing} clusters, and we also explore the
correlation between the scatter in cluster temperature and the scatter
in cluster concentration to establish a general mass-temperature relation that is independent of the dynamical state of the clusters.

\subsection{The $M-T$ Relation for Relaxed Strong Lensing Clusters}
\label{mtrelaxed}

A correlation between cluster mass and cluster X-ray gas temperature in relaxed clusters
is expected as a direct consequence of theoretical arguments.
If a cluster's X-ray gas is in virial and hydrostatic equilibrium,
then the theoretical expectation is that cluster mass scales with X-ray temperature as
$E(z)M_\Delta=A(\Delta)T^{1.5}$, where
$E(z)=H(z)/H_0=\sqrt{\Omega_{\rm m}(1+z)^3 + \Omega_\Lambda}$ for a flat
Universe, $M_\Delta$ is the cluster mass within the radius where
the mean mass density is $\Delta$ times the critical density, and $A(\Delta)$ is the $\Delta$-dependent normalization.

The critical overdensity $\Delta=2500$ is commonly used in cluster
analyses because in the central regions enclosed by $r_{2500}$, {\it Chandra}
cluster temperature profiles can be measured even at high redshifts
(e.g., up to $z=0.9$ in \citealt{AL04.2}).  The overdensity
$\Delta=2500$ is therefore appropriate for our cluster sample, which
extends to $z=0.8$.  Using the overdensity $\Delta=2500$, we can write
the cluster mass-temperature relation in power law form as

\begin{equation}
E(z) \left( \frac{M_{2500}} {10^{14} \, h_{70}^{-1} \, M_\odot} \right) = A \left( \frac{k T}
{5 \, \mathrm{keV}} \right)^\alpha \, .
\end{equation}

Using our sample of four dynamically relaxed lensing clusters given in
\S~\ref{relaxed}, a best fit to the power law $M-T$ relation yields
$A=1.60 \pm 3.42$ and $\alpha=1.43 \pm 1.28$, consistent with the theoretical expectation of
$\alpha=1.5$. Figure~\ref{fig:MT} shows this best-fit relation, for which the RMS scatter is 360$\%$ for all
eight clusters and 500$\%$ for the four unrelaxed clusters.

\begin{figure}[!t]
\begin{center}
\includegraphics[scale=.9]{fig1.eps}
\end{center}
\vspace{-.1in}
\caption{The mass-temperature relation for observed strong lensing clusters.  Unrelaxed clusters (open circles) are not included in the fit, and the relaxed clusters (black points) are fit by a power law with slope $\alpha=1.43$ (black solid line).  The 1$\sigma$ scatter for all eight clusters is large, $\Delta(\log[E(z) M_{2500}])=0.2$ (black dashed lines). Also shown are the other $M-T$ relations for observational samples that use spectroscopic temperatures as we do: 17 weak lensing clusters with $3.6 < T_{\rm s}  \; ({\rm keV}) < 9.8$ (\citealt{HO07.2}; red dotted line), 13 relaxed X-ray clusters with $0.7 < T_{\rm s}  \; ({\rm keV}) < 8.9$ (\citealt{VI06.1}; blue dash-dotted line), 10 relaxed X-ray clusters with $2.2 < T_{\rm s}  \; ({\rm keV}) < 8.3$ (\citealt{AR05.1}; orange dashed line), and six relaxed X-ray clusters with $3.7 < T_{\rm s}  \; ({\rm keV}) < 8.3$ (\citealt{AR05.1}; green long dashed line).  We find that our slope is in agreement with both the theoretical expectation of $\alpha=1.5$ and measurements of $\alpha$ by other observations. For a detailed comparison to these and other estimates of the $M-T$ relation, see Table~\ref{tbl:mtrelation}.
}
\label{fig:MT}
\end{figure}

\begin{deluxetable*}{llllll}
\tablewidth{0pt}
\tablecolumns{6}
\tablecaption{Power Law Fits to the $M-T$ Relation.}
\tablehead{
\colhead{$A$} &
\colhead{$\alpha$} &
\colhead{Method\tablenotemark{a}} &
\colhead{$k T$ (keV)\tablenotemark{b}} &
\colhead{Sample} &
\colhead{Reference}
}
\startdata
$1.60 \pm 3.42$ & $1.43 \pm 1.28$ & SL & $4.6 < T_{\rm s} < 6.7$
& 4 relaxed SL clusters & 1 \\
$2.0\phantom{0} \pm 0.29$ & $1.34^{+0.30}_{-0.28}$ & WL & $3.6 < T_{\rm s} < 9.8$ & 17 WL
clusters & 2 \\
$1.79 \pm 0.07$ & $1.64 \pm 0.06$ & X-ray & $0.7 < T_{\rm s} < 8.9$ & 13 relaxed
clusters & 3 \\
$2.06 \pm 0.10$ & $1.58 \pm 0.07$ & X-ray & $0.6 < T_{\rm m} < 9.3$ & 13 relaxed
clusters & 3 \\
$1.69 \pm 0.05$ & $1.70 \pm 0.07$ & X-ray & $2.2 < T_{\rm s} < 8.3$ & 10
relaxed clusters & 4 \\
$1.79 \pm 0.06$ & $1.51 \pm 0.11$ & X-ray & $3.7 < T_{\rm s} < 8.3$ & 6
relaxed clusters & 4 \\
$1.88 \pm 0.26$ & $1.52 \pm 0.36$ & X-ray & $5.6 < T_{\rm m} < 15.3$ & 5
relaxed WL or SL clusters & 5 \\
$1.97 \pm 0.07$ & $1.54 \pm 0.02$ & Simulation & $T_{\rm m}$ & $M_{2500} > 4 \times
10^{14} \, h_{70}^{-1} \, M_\odot$ clusters & 6 \\
 & & & &  in hydrodynamics
simulation & \\
\enddata

\tablenotetext{a}{Method used to determine the cluster mass, where SL is strong lensing and WL is weak lensing.}
\tablenotetext{b}{Temperature range of the cluster sample, where $T_{\rm s}$
is the spectroscopic temperature and $T_{\rm m}$ is the mass-weighted temperature.}

\tablerefs{(1) This paper; (2) \cite{HO07.2}; (3) \cite{VI06.1}; (4) \cite{AR05.1};
  (5) \cite{AL01.2}; (6) \cite{KA05.1}.}

\label{tbl:mtrelation}
\end{deluxetable*}

\begin{figure}[!t]
\begin{center}
\includegraphics[scale=.9]{fig2.eps}
\end{center}
\vspace{-.1in}
\caption{The correlation between the difference $\Delta T$ between the observed X-ray temperatures and the predicted temperatures from the $M-T$ relation and the difference $\Delta c$ between the measured concentrations and the predicted concentrations from the $c-M$ relation.  The eight strong lensing clusters in our sample are represented, and the solid line shows the best-fit line to the data $\Delta T = (-2.75 \; {\rm keV}) \Delta c -(1.56 \; {\rm keV})$.  The dashed lines show the 1$\sigma$ scatter $\Delta (\Delta T)=0.9$ keV.
}
\label{fig:deltaTdeltac}
\end{figure}

\begin{figure}[!t]
\begin{center}
\vspace{-.1in}
\includegraphics[scale=.9]{fig3.eps}
\end{center}
\caption{The mass-temperature relation, after correcting for the scatter in temperature, for observed strong lensing clusters.  As in Figure~\ref{fig:MT}, open circles represent unrelaxed clusters and black points represent relaxed clusters.  We adjust the temperature of each cluster according to its concentration and the $\Delta T - \Delta c$ relation.  The best-fit $M-T$ relation for relaxed clusters, derived in \S~\ref{mtrelaxed}, is shown as the solid line. The 1$\sigma$ scatter for all eight clusters is $\Delta(\log[E(z) M_{2500}])=0.1$ (black dashed lines), significantly smaller than the scatter in the uncorrected $M-T$ relation (see Figure~\ref{fig:MT}).
}
\label{fig:mtscatter}
\end{figure}

We compare with other observations and simulations of the $M-T$ relation in
Table~\ref{tbl:mtrelation}, including those that used spectroscopic
temperatures $T_{\rm s}$ and those that used mass-weighted
temperatures $T_{\rm m}$.
For cases where the
temperature normalization is not 5 keV and/or the mass scaling is not $10^{14} \, h_{70}^{-1} \, M_\odot$, we recalculate $A$ using the
published slope $\alpha$, a temperature normalization of 5 keV, and a
mass normalization of $10^{14} \, h_{70}^{-1} \, M_\odot$.  To
be conservative, we assume the fractional error in $A$ is unchanged.

The observations we compare span varying temperature ranges, and
there is some evidence that the $M-T$ relation steepens for cooler
clusters (e.g., \citealt{NE00.2,FI01.1}); for example, \cite{AR05.1} find a slope of $\alpha=1.51$ for clusters with $3.7 < T_{\rm s} < 8.3$ keV, which increases to $\alpha=1.70$ for clusters with $2.2 \; \mathrm{keV} < T_{\rm s} < 8.3$ keV.  The temperature range we probe ($4.6 \; \mathrm{keV} < T_{\rm s} < 6.7 $ keV) is likely too small to exhibit a significant change in slope, but we lack a large enough statistical sample to test this properly.

We find that our best-fit slope $\alpha$ is consistent with both
the theoretical expectation and the slopes derived by other
observations and simulations of clusters.  Our best-fit normalization
$A$ is somewhat lower than, but still consistent with, the
normalizations found by the other observations and
simulations. We find that relaxed strong lensing clusters follow the same
$M-T$ relation as relaxed clusters in general.

\subsection{Correlation between the Temperature Scatter and Concentration Scatter}
\label{dTdc}

We have derived an $M-T$ power-law relation for relaxed lensing clusters, but a more general $M-T$ relation including both relaxed and unrelaxed clusters may be possible if we account for the differences in cluster concentrations.  First, we define the virial radius of a cluster as the radius $r_\mathrm{vir}$ at which the average cluster density equals $\Delta_\mathrm{vir}(z)$ times the mean density at the cluster redshift $z$, where $\Delta_\mathrm{vir}(z) \simeq (18 \pi^2 + 82x -39x^2)/(1+x)$ and $x  \equiv \Omega_{\rm m}(z) -1$ \citep{BR98.2}.  Using the scale radius $r_{\rm s}$ of the best-fit NFW profile to each cluster, the cluster concentration is defined as $c_\mathrm{vir} \equiv r_\mathrm{vir} / r_{\rm s}$.

Since more concentrated clusters are expected to form at higher redshifts
(e.g., \citealt{NA97.1}; \citealt{WE02.1}), if the cluster X-ray gas
cools with time there might be a correlation between high cluster
concentrations and low cluster temperatures.  In addition, mergers
with other clusters or groups may deplete the central mass densities in clusters while shock-heating the cluster gas, producing high cluster temperatures for low cluster concentrations.  Here, we analyze whether there is any such correlation between the scatter in temperature and the scatter in concentration for our sample of eight strong lensing clusters.

Cluster concentrations $c_\mathrm{vir}$ and cluster virial masses $M_\mathrm{vir} \equiv M(\leq r_\mathrm{vir})$ are determined by strong lensing measurements for each of the clusters in our sample in \cite{CO07.1}.
The concentration $c_\mathrm{vir}=16$ determined by strong lensing measurements of MS~2137.3$-$2353 is known to be overestimated  because the cluster's dark matter halo is likely elongated along or near the line of sight \citep{GA05.1}, so we instead use the concentration $c_\mathrm{vir}=8.75$ derived from the X-ray mass profile for MS~2137.3$-$2353 \citep{SC07.2}.  We note that if the lensing concentration were used for MS~2137.3$-$2353, Equation~\ref{eq:dtdc} would be $\Delta T = (-0.07 \; {\rm keV}) \Delta c -(0.49 \; {\rm keV})$.

From a sample of 62 galaxy clusters, \cite{CO07.1} find a power-law relation between cluster concentration $c_\mathrm{vir}$ and cluster virial mass $M_\mathrm{vir}$ of
\begin{equation}
c_\mathrm{vir}=\frac{14.5 \pm 6.4} {(1+z)} \left( \frac{M_\mathrm{vir}} {1.3 \times 10^{13} \, h^{-1} \, M_\odot} \right)^{-0.15 \pm 0.13} \; ,
\end{equation}
where $z$ is the cluster redshift.  For each of the eight clusters in our sample, we calculate the difference $\Delta c$ between the measured concentration and the concentration predicted by the above $c-M$ relation.  We also calculate the difference $\Delta T$ between the measured X-ray temperature and the temperature predicted by the $M-T$ relation we determined in \S~\ref{mtrelaxed} for the four relaxed clusters.

Figure~\ref{fig:deltaTdeltac} shows the results of these $\Delta T$
and $\Delta c$ calculations.  The best-fit line to the data is
\begin{equation}
\Delta T = (-2.75 \; {\rm keV}  \pm 0.07 \; {\rm keV}) \Delta c -(1.56 \; {\rm keV} \pm 0.49 \; {\rm keV}) \; ,
\label{eq:dtdc}
\end{equation}
suggesting that indeed higher (lower) temperature clusters tend to have lower (higher) concentrations.

\subsection{The $M-T$ Relation for All Strong Lensing Clusters}

Using the relation between the scatter in cluster temperature
and the scatter in cluster concentration for the eight strong lensing
clusters (\S~\ref{dTdc}), we adjust for the apparent dependence of cluster temperatures on
cluster concentrations.  We use $\Delta c$ for each cluster to calculate its
corresponding $\Delta T$ from the best-fit relation given in Equation~\ref{eq:dtdc}.  We then subtract this $\Delta
T$ from the measured temperature to obtain a corrected temperature $T_{\rm corr}$, and we illustrate the resultant
temperature-corrected $M-T$ relation in Figure~\ref{fig:mtscatter}.
The figure also shows the relation we derived in \S~\ref{mtrelaxed} for the four
relaxed clusters, where $A=1.60$ and $\alpha=1.43$.

We find that cluster concentration, mass, and X-ray temperature are
tightly correlated, and as a result incorporating the $\Delta T - \Delta c$
relation significantly reduces the scatter in the $M-T$ relation.
Comparing Figure~\ref{fig:mtscatter} to Figure~\ref{fig:MT}
underscores the impact of our temperature correction in reducing the
scatter in the $M-T$ relation.  The temperature correction reduces the
RMS scatter for all eight clusters by a factor of 6, from 360$\%$ to
60$\%$, and more significantly, reduces the RMS scatter for the four unrelaxed clusters by a factor of 30, from 500$\%$ to 15$\%$. (The RMS scatter for the four relaxed clusters increases from 26$\%$ to 83$\%$, possibly because the temperatures we use do not correct for cool cores at the cluster centers.)
With the temperature correction, even unrelaxed clusters follow the
$M-T$ relation we originally derived using only the relaxed clusters
(\S~\ref{mtrelaxed}).  Therefore, we suggest this temperature
correction as a tool for establishing a universal $M-T$ relation that
applies to all galaxy clusters regardless of their dynamical state.

The error in the measurement of $\sigma_8$ from cluster counts depends
directly on the error in the cluster $M-T$ relation; for example, a
25$\%$ 1$\sigma$ uncertainty in the zero point of the $M-T$ relation corresponds
to a $10\%$ 1$\sigma$ uncertainty in $\sigma_8$ \citep{EV02.1}.  Consequently,
 we find that the temperature correction not only reduces the
scatter in the $M-T$ relation, but also significantly reduces the error in the
corresponding measurement of $\sigma_8$.

An alternate cluster scaling relation that also has lower scatter than the traditional $M-T$ relation is the $Y_{\rm X} - M_{500}$ relation \citep{KR06.1}.
Here, $M_{500}$ is the cluster mass within the radius $r_{500}$ enclosing an overdensity of 500 relative to the critical density, $Y_{\rm X}=M_g T_{\rm X}$, $M_g$ is the cluster gas mass within $r_{500}$, and $T_{\rm X}$ is the mean spectral X-ray temperature of the cluster.  However, this scaling relation is limited by the assumptions that the gas is both spherically distributed and in hydrostatic equilibrium.  Our scaling relation offers the advantage that it is based on lensing mass estimates that are free of these assumptions.

\begin{deluxetable*}{lllll}
\tablewidth{0pt}
\tablecolumns{5}
\tablecaption{BCG luminosities.}
\tablehead{
\colhead{Cluster} &
\colhead{BCG\tablenotemark{a}} &
\colhead{$L_\mathrm{K, BCG}$} &
\colhead{$L_\mathrm{K, passive, BCG}$} &
\colhead{Reference} \\ & &
\colhead{$(10^{11} \, h_{70}^{-2} \, L_\odot)$} &
\colhead{$(10^{11} \, h_{70}^{-2} \, L_\odot)$} &
}
\startdata
ClG~2244$-$02 & & $1.03 \pm 0.09$ & $0.96 \pm 0.09$ &  1 \\
Abell~370 & G1 & $1.5\phantom{0} \pm 0.1$ & $1.3\phantom{0} \pm 0.1$ &  \\
3C~220.1 &  & $6.4\phantom{0} \pm 0.4$ & $5.3\phantom{0} \pm 0.3$ &  \\
MS~2137.3$-$2353 & & $8.98 \pm 0.09$ & $0.84 \pm 0.08$ &  \\
MS~0451.6$-$0305 & & $4.3\phantom{0} \pm 0.3$ & $3.7\phantom{0} \pm 0.3$ &  2 \\
MS~1137.5$+$6625 & & $15\phantom{.0} \pm 2$ & $11\phantom{.0} \pm 1$ &  \\
Cl~0939$+$4713 & G1 & $1.9\phantom{0} \pm 0.2$ & $1.7\phantom{0} \pm 0.2$ &  3 \\
ZwCl~0024$+$1652 & $\#$362 & $1.69 \pm 0.07$ & $1.51 \pm 0.06$ &  4, 5 \\
\enddata

\tablenotetext{a}{See \cite{CO06.1} for identification of the galaxies
by name.}

\tablerefs{(1) \cite{BA82.2}; (2) \cite{EL98.1}; (3) \cite{DE03.1}; (4) \cite{KN03.1};
  (5) \cite{MO05.1}.}

\label{tbl:lum}
\end{deluxetable*}

\section{BCG Properties}
\label{bcgprop}

In addition to the interdependencies of many cluster properties, properties of the BCG have also been shown to correlate with the host cluster.  Here we identify the BCG in each of our clusters, measure the luminosity of each BCG, and examine the correlation between BCG luminosity and host cluster mass for our strong lensing sample.

\subsection{BCG Determination}
\label{bcg}

We select each cluster's BCG as the brightest member galaxy.  Each BCG corresponds to the lens galaxy or one of the lens galaxies used to determine the cluster mass distribution in \cite{CO06.1}.  When multiple lens galaxies were used to model a single cluster, we identify which of the lens galaxies is the BCG in Table~\ref{tbl:lum}, and we also note references that confirm the BCG selection.

\subsection{BCG Luminosity Determination}
\label{light}

For each cluster we have {\it HST} imaging taken in some combination of the
filters F450W, F555W, F675W, F702W, and F814W. Using Source EXtractor
\citep{BE96.1}, we measure MAG\_AUTO magnitudes for the BCG galaxies.
We estimate the
magnitude uncertainties by adding in quadrature the error in the measured flux
and the estimated background subtraction error, which is the product of the
area of the extraction aperture and the RMS variation of the subtracted
background flux.  We calculate the BCG luminosities using the available
photometry in an observed band as the normalization factor on two types of
spectral energy distribution templates, and then compute the rest-frame
magnitudes and luminosities in several bands including {\it K}-band.  The templates we
use are calculated from the
\cite{BR03.1} stellar population synthesis models with a Salpeter
initial mass function.  The first we use is a fixed-age 10 Gyr old simple
stellar population, and the second is for a simple stellar population with
an age given by an assumed formation redshift of $z=3.0$. The latter
enables an estimate of the passively-evolved BCG luminosity.

\section{The BCG Luminosity - Cluster Mass Relation}
\label{lm}

\begin{figure}[!t]
\begin{center}
\includegraphics[scale=.9]{fig4.eps}
\end{center}
\vspace{-.1in}
\caption{The correlation between {\it K}-band BCG luminosity and cluster mass for our sample of strong lensing clusters.  Uncorrected luminosities (black points) are fit by the solid line, while luminosities corrected for passive evolution (open circles) are fit by the dashed line.  For comparison, the \cite{LI04.3} $L-M$ relation for the general cluster population is shown as the dotted line.  Our best-fit power laws are significantly steeper than that of \cite{LI04.3}, hinting that BCGs in lensing clusters may have different formation histories than BCGs in typical clusters. }
\label{fig:lmlinmohr}
\end{figure}

Although it is still unclear how BCGs form, conventional formation scenarios include galactic
cannibalism, cooling flows, and mergers during cluster formation (\S~\ref{intro}).
The evolution of the luminosity of the BCG with the mass of the cluster may distinguish between these models and offer insight into the formation of BCGs.
Semianalytic and numerical simulations of structure formation suggest
a tight correlation between BCG luminosities and cluster masses (e.g.,
\citealt{SO99.1,CO00.1}), and we can parameterize such a correlation
between {\it K}-band BCG luminosities and cluster masses $M_{200}$ by the power law

\begin{equation}
\frac{L_\mathrm{K, BCG}} {10^{11} \; h_{70}^{-2} \; L_\odot} = B \left( \frac{M_{200}} {10^{14} \; h_{70}^{-1} \; M_\odot} \right)^\beta \; .
\end{equation}

Here, we examine the relation between BCG luminosity and cluster mass for clues about the
formation histories of BCGs in strong lensing clusters and how their
formations may differ from the general BCG population.  We represent
the general BCG population with the \cite{LI04.3} study of 93 BCGs at $z \leq 0.09$ in the Two Micron All Sky Survey (2MASS).

For an accurate comparison to the $L-M$ relation
\cite{LI04.3} find from 2MASS, we follow their definition of BCG
luminosity.  \cite{LI04.3} measure BCG luminosities in the {\it K}-band using 20 mag arcsec$^{-2}$ isophotal elliptical
aperture magnitudes for 2MASS, called K20 magnitudes.  Similarly, we
convert to the {\it K}-band (see  \S~\ref{light}) and measure BCG
magnitudes using SExtractor's MAG\_AUTO function \citep{BE96.1}, which
has good agreement with 2MASS K20 total magnitudes for sources such as
BCGs that are bright and extended \citep{EL06.1}.  We then convert the
magnitudes into {\it K}-band luminosities as described in
\S~\ref{light}. The resultant {\it K}-band BCG luminosities, along
with the luminosities corrected for passive evolution, are given in Table~\ref{tbl:lum}.

Figure~\ref{fig:lmlinmohr} illustrates the correlation between BCG luminosities and
cluster masses $M_{200}$. We find
the best-fit power law to the data is given by $B=0.97 \pm
0.17$ and $\beta=0.48 \pm 0.09$ for all strong lensing clusters (solid
line in Figure~\ref{fig:lmlinmohr}) and $B=0.93 \pm 0.18$ and $\beta=0.39 \pm 0.10$ for all strong
lensing clusters when the BCG luminosities are corrected for passive
evolution (dashed line in Figure~\ref{fig:lmlinmohr}).   The similarity of these two results implies that the passive evolution of BCG
luminosities with redshift has little effect on the $L-M$ relation,
and more generally
there is no evidence for evolution in the $L-M$ relation from
$z\sim1$ to $z\sim0$ \citep{BR08.1}

For comparison, \cite{LI04.3} find a
best-fit power law of $B=4.9 \pm 0.2$ and $\beta=0.26 \pm 0.04$
(dotted line in Figure~\ref{fig:lmlinmohr}), which is consistent with the slopes found by
analytic estimates and cosmological simulations of the growth of central galaxies.  Using the
galaxy-dark matter correlation function to determine host dark matter
halo masses for observational catalogs of galaxies, \cite{CO05.1} find $L
\propto M_{200}^{<0.3}$ for halo masses $\gtrsim 4 \times
10^{13} \; h^{-1} \; M_\odot$.  Similarly, \cite{VA06.1} determine a
correlation of $L
\propto M_{100}^{0.28}$ when they combine the subhalo mass distribution
derived from simulations with an empirical galaxy luminosity function.
They also find little dependence of the $L-M$ relation on waveband.

From their slope of $\beta=0.26$, \cite{LI04.3} conclude that while
other cluster members may merge with BCGs and increase BCG
luminosities, such effects are not sufficient to fully account for the
growth in $L_\mathrm{K, BCG}$ with cluster mass.  Instead,
\cite{LI04.3} suggest that BCGs must grow mainly through mergers with
other BCGs brought in when the host galaxy cluster merges with other
groups or clusters.  In addition to the many hierarchical structure
formation simulations and models that support this scenario (e.g.,
\citealt{ME85.1, DU98.1, BO06.1}), there are also observations of a
pair of $\sim L^{*}$ elliptical galaxies merging to build up the BCG
in a rich cluster at $z=1.26$ \citep{YA02.1}.

Our slope $\beta$ is 50$\%$ (when luminosities are corrected
for passive evolution) to 85$\%$ (when luminosities are not corrected
for passive evolution) steeper than that of \cite{LI04.3}, hinting
that strong lensing clusters may undergo more mergers with groups and
clusters, or merge with more massive groups and clusters, than the
average cluster.  Both more mergers and mergers with more
massive systems could account for the initial evidence for an increase in
$L_\mathrm{K, BCG}$ with cluster mass we find in strong lensing
clusters, and would also be consistent with simulations that suggest
strong lensing clusters are dynamically more active than the general
cluster population \citep{BA96.2}.  However, the scatter in our $L-M$ relation is significant, and a larger sample of strong lensing clusters is necessary to draw definitive conclusions about the formation histories of strong lensing clusters.

\section{Conclusions}
\label{conclude}

We have determined the scaling of cluster mass with cluster temperature and the scaling of BCG
luminosity with cluster mass for eight observed strong lensing
galaxy clusters imaged with {\it HST} and at redshifts $0.3 < z < 0.8$.  We explored cluster
concentrations as a means of reducing the scatter in the $M-T$
relation and
enabling more precise constraints on cosmological parameters, and we
used the $L-M$ relation as an indicator of the formation
histories of strong lensing BCGs and clusters.
Our main results are:

\begin{enumerate}

\item  The best-fit cluster mass-temperature relation for our four
dynamically relaxed strong lensing clusters is
\begin{equation}
\label{eq:mt}
E(z) \left( \frac{M_{2500}} {10^{14} \, h_{70}^{-1} \, M_\odot}
\right) = 1.60 \pm 3.42 \left( \frac{k T}
{5 \, \mathrm{keV}} \right)^{1.43 \pm 1.28} \, ,
\end{equation}
which is consistent with the theoretical expectation of the $M-T$ relation for relaxed clusters, as well as the $M-T$ relations
determined by other observations and simulations.  We find that
relaxed strong lensing clusters do not deviate from the $M-T$ relation
for the general population of relaxed clusters.

Significantly, we find an inverse correlation between cluster temperature and
cluster concentration that, when incorporated into the
$M-T$ relation, reduces the $M-T$ scatter by a factor of 6, from 360$\%$ to 60$\%$.  By
correcting cluster temperatures according to the
temperature-concentration relation, we find that the
$M-T$ relation given in Equation~\ref{eq:mt} describes not only the
relaxed strong lensing clusters, but the entire cluster population
regardless of dynamical state.  Specifically, the scatter in unrelaxed clusters decreases by a factor of
30, from 500$\%$ in the uncorrected $M-T$ relation to 15$\%$ in the
temperature-corrected $M-T$ relation.  Incorporating concentration
effects into the $M-T$ relation tightens the $M-T$
relation for all clusters, which in turn
reduces the error in the determination of $\sigma_8$ from
cluster counts.  Whereas accurate cluster determinations of $\sigma_8$ were previously made only with relaxed clusters, concentrations enable the inclusion of unrelaxed clusters.  The larger cluster samples possible with the inclusion of unrelaxed clusters offer yet more precise $\sigma_8$ estimates from cluster observations.

\item The best-fit relation between BCG luminosity and cluster mass for
our sample of strong lensing clusters is
\begin{equation}
\frac{L_\mathrm{K, BCG}} {10^{11} \; h_{70}^{-2} \; L_\odot} = 0.97
\pm 0.17 \left( \frac{M_{200}} {10^{14} \; h_{70}^{-1} \; M_\odot}
\right)^{0.48 \pm 0.09} \; ,
\end{equation}
which is $\sim 85\%$ steeper than the correlations predicted for non-strong-lensing clusters by other
observations, theory, and cosmological simulations.  This result
supports the current evidence that BCGs are built up through mergers
with massive galaxies in other groups and clusters, and also hints that strong
lensing clusters may have more active merging histories than
typical clusters.  A larger sample of strong lensing clusters might enable more definite conclusions about the formation histories of strong lensing clusters.

\end{enumerate}

Accurate cluster mass measurements and full use of the
range of cluster property interdependencies are key components in the calibration of
clusters as tracers of cosmological parameters.  As we have shown,
gravitational lensing enables the most direct measurements of cluster
mass, without assumptions about the cluster's dynamical state that are
inherent in other methods.  We have also shown that the correlation
between cluster temperature and concentration can significantly reduce the
scatter in the cluster $M-T$ relation, enabling more precise
estimates of $\sigma_8$.  It may be that other cluster scalings can be
effectively combined to reduce the error on additional cosmological
parameter estimates.

\acknowledgements J.M.C. acknowledges support of this work by a National Science
Foundation Graduate Research Fellowship. The work of L.A.M. was
carried out at the Jet Propulsion Laboratory, California
Institute of Technology, with the support of NASA ATFP08-0169. P.N. would like to thank the Radcliffe Institute for Advanced Study and the Center for Astrophysics (CfA)
for providing an intellectually stimulating atmosphere that enabled this work.

\bibliographystyle{apj}

redpajama_set_name: RedPajamaArXiv


I wanted to start with the biggest tip I ever got concerning writing.
Yes, read anything and everything you can find in your genre, be it romance, sci-fi, western, whatever... read and absorb. Am I saying to copy? No, no, no. But the more you read, you'll see what works, what doesn't work, what publishers are buying.
Okay, so that sounds silly or maybe what you might call obvious. You'd be surprised. I've met plenty of aspiring writers who don't read. Their work reflects that. I've also met and become friends with MANY PUBLISHED writers who READ ALL THE TIME. They do it to improve their craft, to see what's out there, and to find new voices in writing.
So the best advice I can give anyone who wants to start writing is to read and read widely.
I sent a short story to an editor a while back. While you may recall that the editor told me: thanks, but resubmit when you have the bugs worked out.
Well, I worked out those bugs. I fixed the beginning and I think, not totally sure (Who really ever is?), that the editor will like it. She liked it enough to ask for a resub, which I've heard is rare for her. Fingers crossed!
Also, I submitted another longer story about my Air Force soldiers to WRP. I'm hoping for good things. I really feel strongly about the emotional quality of this story and hope it will resonate with readers. We shall see.
So off my soapbox and back to the bat cave.
And good luck with your submissions!
Sure do have a bat cave! It's where I work on my bat words like Ponk, Zowie, and Zink!
I'll put the kit in the mail so you can make your own.


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text:
Q: Unity Switched weapon not syncing PUN 2 I managed to get my shooting synchronised however i cant figure out how to sync weapon switching (using the same method, rpc)
the problem is that whenever i switch weapons, it doesnt show on my second screen.
public class WeaponHolder : MonoBehaviour
{
    PhotonView view;

    public int selectedWeapon = 0;

    void Start()
    {
        view = GetComponent<PhotonView>();
        if(!view.IsMine)
        {
            return;
        }
        SelectWeapon();
    }

    void Update()
    {
        if(!view.IsMine)
        {
            return;
        }
        if(FindObjectsOfType<weaponScript>()[0].isReloading == true)
        {
            return;
        }
        else
        {
            view.RPC("switchWeapon", RpcTarget.All);
        }
    }

    [PunRPC]
    public void switchWeapon()
    {
        if(!view.IsMine)
        {
            return;
        }
        int previousSelectedWeapon = selectedWeapon;
        if(Input.GetAxis("Mouse ScrollWheel") > 0f)
        {
            if(selectedWeapon >= transform.childCount - 1)
            {
                selectedWeapon = 0;
            }
            else
            {
                selectedWeapon++;
            }
        }

        if(Input.GetAxis("Mouse ScrollWheel") < 0f)
        {
            if(selectedWeapon <= 0)
            {
                selectedWeapon = transform.childCount - 1;
            }
            else
            {
                selectedWeapon--;
            }
        }

        if(previousSelectedWeapon != selectedWeapon)
        {
            SelectWeapon();
        }
    }

    public void SelectWeapon()
    {
        int i = 0;
        foreach (Transform weapon in transform)
        {
            if(i ==  selectedWeapon)
            {
                weapon.gameObject.SetActive(true);
            }
            else
            {
                weapon.gameObject.SetActive(false);
            }
            i++;
        }
    }
}

(used brackeys' tutorial for weapon switching)
i did the exact same with my shooting script and that worked, i have a photon view component on my gameobject where i have this script attached to it

A: Within an RPC you wouldn't want to check
if(!view.IsMine){ return; }

then what would be the purpose of sending this as RPC to everyone? You could simply call this only on your device ;) you want this happen on all other clients as well.
You will want to restructure your methods and execute SwitchWeapon only on your device directly without an RPC and then rather pass on SelectWeapon(int) via RPC to everyone and pass in the new index.
void Update()
{
    if(!view.IsMine)
    {
        return;
    }

    if(FindObjectsOfType<weaponScript>()[0].isReloading)
    {
        return;
    }

    switchWeapon();
}

private void switchWeapon()
{
    if(!view.IsMine)
    {
        return;
    }

    var scroll = Input.GetAxis("Mouse ScrollWheel");
    if(scroll > 0f)
    {
        selectedWeapon = (selectedWeapon + 1) % transform.childCount;
        view.RPC(nameof(SelectWeapon), RpcTarget.All, selectedWeapon);
    }
    else if(scroll < 0f)
    {
        selectedWeapon--;
        if(selectedWeapon < 0)
        {
            selectedWeapon = transform.childCount - 1;
        }

        view.RPC(nameof(SelectWeapon), RpcTarget.All, selectedWeapon);
    }
}

[PunRPC]
public void SelectWeapon(int newWeapon)
{
    int i = 0;
    foreach(Transform weapon in transform)
    {
        weapon.gameObject.SetActive(i == newWeapon);
    }
    i++;
}

and also in Start do
view.RPC(nameof(SelectWeapon), RpcTarget.AllBuffered, selectedWeapon);

redpajama_set_name: RedPajamaStackExchange