Inside Racing – Saturdays at 7:00 A.M. PST on KEIB 1150 AM (Los Angeles). Hosted by JASON LEVIN with handicappers Jay Friedlander, Steve Pollack and Thoro-Graph's Alan Benowitz. Streams live at racingjason.com and patriot.la. Podcasts available at patriot.la immediately after the show.
The Roger Stein Show – Saturday and Sunday 8:00 to 9:00 A.M. PST on KLAA 830 AM. Streams live and on archive at rogerstein.com.
Thoroughbred Los Angeles – Saturdays 9:00 to 10:00 A.M. PST on KLAA 830 AM. Hosted by JAY PRIVMAN airs at am830klaa.com, drf.com, todaysracingdigest.com.
Thoroughbred Los Angeles – Sundays 9:00 to 10:00 A.M. PST on KLAA 830 AM. Hosted by MIKE WILLMAN and KURT HOOVER airs at am830klaa.com, drf.com, todaysracingdigest.com.
At the Track with Sam Spear – Saturday from 7:00 to 8:00 A.M. PST on KNBR 680 AM (San Francisco).
At the Races with Steve Byk – Monday through Friday 10:00 to 1:00 P.M. PST on Sirius 93 and XM 209. The live show is also available at thoroughbredracingradionetwork.com as well as podcasts and archives of the show.
Down the Stretch with Dave Johnson and Bill Finley – Saturdays from 7:00 to 10:00 A.M. PST on Sirius 93 and XM 208. Call in your questions to (866) 900-6451.


Theatrical Heritage: Challenges and Opportunities. Eds. Forment, Bruno; Stalpaert, Christel. Leuven: Leuven University Press, 2015. 195–205.
Posted in 2015, English and tagged canonisation, contemporary theatre, criticism, digital humanities, Etcetera, text-mining on May 11, 2015 by tcrombez.
Etcetera nr. 135 (dec. 2013). 8-13.
Posted in 2013, Nederlands and tagged Carlos Tindemans, Etcetera, Living Theatre, neo-avant-garde, reception studies on January 15, 2014 by tcrombez.
Posted in 2006, Nederlands and tagged Etcetera, Friedrich Nietzsche, political art on May 25, 2008 by tcrombez.


text:
Narragansett police, SPCA investigating after dog found in river, shot in the head
NARRAGANSETT -- The Rhode Island Society for the Prevention of Cruelty to Animals is offering a $500 reward for information leading to the arrest and conviction of the person responsible for the death of a dog found in the Narrow River, with an apparent gunshot wound to the head.
The dog appears to have been an adult male terrier-type dog, about 5 to 6 years old. The dog appeared to have had a severe skin infection that would have been immediately recognizable to anyone who knew him, the SPCA said.
"We would strongly encourage the owner or the person responsible for this act to come forward and identify themselves," Joe Warzycha, the SPCA president, said in a news release. "We will continue to investigate this matter until all avenues are exhausted and any help from the general public would be greatly appreciated."
Due to the condition of the dog, the SPCA did not make photos available, but photos can be made available to anyone who believes they have credible information.
Anyone with information is asked to call Detective Brent Kuzman of the Narragansett police at (401) 789-1091, ext. 320, or Special Agent Earl Newman of the SPCA at (401) 438-8150, ext 2.
© 2021 www.providencejournal.com. All rights reserved.

redpajama_set_name: RedPajamaCommonCrawl


text:
Posted in Idol: Season 12
Final six perform
ventboys April 13, 2013 Leave a comment
First up was Burnell's ouster. Idol's history tells us that Burnell won't ever be heard from again in the mainstream, and that's probably 98% the expected result, but there is something special, and very pleasing, about being around this kid. Even if he doesn't defy the odds, he should be able to carve out a nice living as a singer, and as a personality. I like him enough to keep tabs on him, and I generally only keep tabs on a couple of contestants from each year. If you like Burnell as much as I like Burnell, I'll keep you posted. Lets get to the show.
The singers, the songs:
Quickly, the contestants and how they engage the audience:
Angie- Selling Tupperware
Amber- Winking at the cute boy across the room
Lazaro- Hello. My name is Inyego Montoya. You killed me father. Prepare to die.
Kree- Omg!! roflmao, it's so good to see you :)
Janelle- Kathy Lee Gifford with a head injury
Candice- Sweetly skeptical, like David Cook was
I'm going to recap both of their performances together. It's Friday and the internet has already weighed in, so I'll mention that when it comes up.
Angie: Forget the first song, that wasn't a good fit and she sang it ok. Her second song will land in the top ten of my end of the year songs. Cynics won't like it, but cynics don't like Idol in the first place. The cynics can eat me; Angie made herself a nice little memory.
Aside– Angie needs to stop looking directly into the camera all the time. Not to be gross, but nothing ruins a good porno like the girl looking into the camera. Fourth wall violations are fine for comedy, but not for art. Passion. Music is passionate, isn't it? It is to me. I don't want them constantly reminding me that they know I'm watching; I want them lost in the moment.
Amber: It's a tribute to how good the others singers are that Amber isn't dominating the competition; she is every bit as good as Crystal, or Jordin, or Carrie and Kelly were when they were on the show. She was second to last, which means fifth, this week. Why?
My best guess is that the judges overgushed a little, giving her fans a false sense of security and her rivals an extra push against her. I don't believe she is the fifth most popular singer; I think she's either fourth or third right now, well behind Kree and Candice, fighting with Angie and holding Janelle off. It's a sick, talented group, isn't it?
Lazaro: It all came crashing down on the kid tonight. He was shaky last week, and he crumbled this week. Siobhan, among others, used to talk at length about how rough it can be to read your reviews online. She stopped using the internet once she reached the semifinals, because (paraphrasing) for every good review there are two trolls who get off on telling you how much you suck; and it's almost impossible to avoid the reviews if you are online. I think Laz got caught up in reading his reviews, and like that big black bowling ball thing the hobbits looked into (was it Merry or Pippin?), it sapped his confidence like he was a replacement referee in the NFL. Don't cry for Laz Argentina, though. He'll have a nice career, as sort of a Latino version of Bill Murray's lounge singer. Vegas will love him (or Reno, lets be real).
Kree: It always feels so unfair when I compare her to Carrie Underwood, but listen back to her Bacharach performance and tell me that you could tell them apart with your eyes closed. In her defense, I don't think Kree was consciously imitating Carrie tonight. I think she was just singing the song, and it sounded like that. The original singer, Jackie DeShannon, sounded like that when Carrie was in diapers. Had Carrie just kept waiting tables and never auditioned, Kree would probably have sung the song exactly the same way.
Backing that up with Sammy Smith's version of "Help Me Make It through the Night" was a bit of overkill, but Kree was subtly just that much different from the original to make it her own version. She sang it beautifully, as we should expect her to.
Janelle: Janelle didn't suck, she was fairly average – but average singing brings Lazaro back into play. Janelle should thank her maker every morning that she was born a white girl with a southern accent; that's just about the only thing that gives her a voting base against Amber and Candice, who are far superior singers, and Angie, who is even whiter and bible belty than she is.
Aside: I left the country in August 1990, and I didn't get back until the end of March, 1991. While I was away, some inbred goat roper named Garth Brooks had a couple of hits. I left knowing "Not Counting You" and "If Tomorrow Never Comes", but that was pretty much it. I was in a band over on the coast, and we kept up with the new stuff pretty well. When I got back from overseas and rejoined the band, we played "Friends in Low Places" the first night. At the end of the song I told Denny "Hey, that's a cool song! Who does it?" He looked at me funny, and started playing the opening chords to "The Dance". He looked back at me and said, "Do you recognize this one?"
I didn't. I had never heard of it.
Candice: The internet gadflies are asking whether Candice's last song was the best Idol song ever. That's an easy question; the answer is no. Adam Lambert, Carrie/Kelly/JHud/Haley, Fantasia, Clay, Siobhan's Paint it Black…. I might see it as top 10-20 depending on criteria. Was it the best this year? I'll say this; I can't think of anything better, and the few that I could toss against it were mostly other performances by Candice. This probably means that she's going to finish second; think about how many times the singer with the most strong performances has finished second: Clay, Bo maybe, Kat, Archie, Adam, Crystal, Jessica; roughly half the time the best singer will finish second.
Laz is gone; seeya (hear ya) in the Elevators, kid.
Power Rankings:
5: Amber- It's a strong last place – she still has a puncher's chance of winning
4: Janelle- She can still win if she doesn't pick a horrible song at the wrong time
3: Angie- Look away from the camera – and she can get back in contention
2: Candice- Is she Jordin, or Crystal?
1: Kree- This year's version of the WGWG, I personally think she's much cuter than the last one
Finals – season 12
Lets hear it – the first ten ladies
Final eight perform
← Final seven perform
Final five perform →


The Harmful Algal Bloom panel will bring together leaders from the coastal tourism, the oyster farming industry, and academia to discuss threats to our coastal communities and economies caused by increasing frequency harmful algal blooms in our region of the Gulf of Mexico. The panel will discuss the types and causes of harmful algal blooms and their consequences from human health and economic perspectives. Industry needs will also be discussed.


Recently, my father died of cancer. And although this was sudden (and yet protracted, as modern death tends to be), and afforded little time to 'prepare' – he left behind a vast body of work through which one might posthumously get to know him better. In life he produced (writing and drawings mostly) constantly, though this fact could only really be construed; he was also what one might describe as pathologically modest – although 'modest' is surely too banal a word for something so holistic in its negativity. Modesty as we colloquially practice it, often suggests a veil of negativity – a loose-fitting and perhaps deliberately not-very-convincing disguise for a genuine pride beneath, a cosset for both the subject and their audience. With dad, it's clear that this was performed almost completely antithetically. For him, modesty was the positivist pall (albeit folded over, shrivelled), behind which lurked not a faithful pride but a truthful and terrible void, a seemingly insurmountable negativity that prevented his ever admitting – to himself, let alone to us, his family – that he was, in fact, good – brilliant. This fact, at least, is beyond objective question. We have all known it for years. He was and always was a genuine and extraordinary talent whose work, glimpsed behind fast-closing cupboard doors and plan chest drawers, was utterly tantalising.
Of course, he knew that as soon as he died we would have to look. Without him standing guard, it was only a matter of time. We would joke about this around the dinner table, in the manner that one can only joke about something so absurdly distant as a death. He would confess, when pushed to recount his day, to the predictable decline of a drawing he was working on; or he might mutter something about such and such anecdote being worthy of going in the diary – and we would pounce on him, hungry for the slightest crumb of insight into his creative world. The diary in particular took on near mythical proportions. He had, we knew, been keeping it since he was sixteen. We also knew about the cupboard he kept every volume of it in – beside the airing cupboard and above his hoard of drawings. Teetering hardbacks, jostling for space. Beyond that, who knew? The joke of death only increased at the ludicrous prospect of ever reading it; his death made even more unimaginable because of the Herculean task it would bestow on us, his poor but ardent, posthumous readers.
This proves too much. The conditions of our admittance having been met, looking through the diary is very difficult. Unlike the raft of drawings (which we rifle through with awe, grinning – dividing, selecting favourites; gifting some, framing some – all of them tangible), the colossal diary is almost completely insoluble. Where does one begin? At the beginning? At the birth of his first child? Marriage? Or is it only manageable in fragments? – aphoristic nuggets and sound bites chiselled off the monolithic whole and savoured as the persistence of a perspective from when he was alive: one dazzling glimpse at a time. I discovered very quickly that I was incapable of browsing a volume without desperately searching for my name – seeking, as a mourner might, some sort of intimate correspondence with the dead; to find a loving consolation, I suppose. A mistake of course, demonstrating perfectly the significant problems with using a diary as a medium for remembrance: Alighting on my name, I read the sentence either side. It describes a fifteen-year-old me dashing out to the pub immediately after dinner, deferring some family obligation. Dad writes (and this isn't a direct quote): "nothing gets in the way of one of Edward's nights out". A mild expression of grievance, but it knocked me for six. And I came rushing to the devastating conclusion that, in actual fact, he had hated me; resented me, even. A preposterous inference from something so banal, perhaps (and one that surely belies the unpredictability and inanity of manifest grief), but it nevertheless shattered any illusions I might have had regarding the contents of his diary. Herein are his truths, all of them. From domestic to pitch black. And this momentary insight, regardless of its triviality, lays bare this fact like a wound. The loss of an ideality is something that, so soon after a death, seems unbearable. For now, in the most part, retrieving and maintaining a memory from before – before the illness in particular – is of paramount importance, regardless of its accuracy. In this way I am for now resigned to and comforted by nostalgia.
The only part of dad's diaries my mum, brother and I have so far truly read and understood are the slim notebooks he kept throughout his illness, written almost daily right up until his death. They are meagre compared to their healthy, voluminous antecedents – but they are all the more poignant for it. Much like the rest of his diary, they are brutally, painfully honest, describing in astonishingly uninhibited terms, his terrible decline. Our ability to approach them lucidly is, however, singular in its calm. For although they are certainly no less unflinching in their confessional than the rest of his diaries, they represent a parallelism to our own perspectives that could only really occur under such horrible circumstances. His increasing infirmity meant a steady and inexorable relinquishing of his own agency – perhaps the most devastating blow for so private, so independent a man; a betrayal of soul by body, he was stripped bare, so that the truths previously kept subterranean in the diaries were exposed to the day and to our frightened gaze; as well as to the cold scrutiny of myriad doctors, nurses and orderlies. The inscription of this betrayal, in the diary as on his body, is very, very painful to read – but, crucially, not impossible. In fact, for me at least, it is almost cathartic. In his chronicling of his illness and his desperately reluctant capitulation to the indignity of dependence, he affirms his agency rather than resigns it. The writing of the diary (as well as the drawings that form an appendix to it) up until the bitter end is as an act of resistance, of defiance. These notes transcend their subject matter precisely because of that subject's objective and all-conquering ubiquity – both through it having been unavoidably witnessed by others, and in the awful, universal pervasion of cancer. He is documenting something that is happening to him – not a life led. He is not in control, as no one is in control of their death, but as he approaches it he has the skill and the dignity to record it with humour, irony, sadness, joy and humanity. And, although he would have found this very hard to admit, I think he knew this.
The view from the hospital bed, a drawing from the back of the diary.


text:
Q: Strip out referers from script src I'm doing a remote script-src
<script src="http://thirdparty.com/test.js"></script>

I don't want to send my http referer headers to thirdparty.com. How do I do it?

A: You would have to proxy the request for the script through your own server. For example:
<script src="stripreferrer.php?url=http%3A%2F%2Fthirdparty.com%2Ftest.js"></script>

Then, your server-side code would make the HTTP request sans referrer code, and pass the response to the client.

A: The answers from 2013 are obsolete: you can do it by setting a referrer policy on your webpage. For example, if you have
<meta name="referrer" content="origin">
on your page, then any <script src="..."> resources fetched from that page (after that line) will send only the origin and not the full URL. Other options include "no-referrer".
See http://caniuse.com/#feat=referrer-policy for status of adoption by browsers: as of Sep 2016 it's supported by most major non-IE browsers. This older blog post on the Mozilla Security blog may be worth reading if you prefer not to read the standard.

A: This is part of the HTTP protocol. You cannot control this using HTML or JavaScript.

redpajama_set_name: RedPajamaStackExchange


text:
Paveway IV je přesně naváděná puma typu vzduch-země od společnosti Raytheon. Jde o nejnovější přírůstek ze série bomb Paveway a její vývoj začal v roce 2003.

Vlastnosti
Paveway IV vznikla přidáním systému navádění a řídících ploch k tělu tzv. "hloupé" (neřízené) pumy typu Mark 82. Hlavní zdokonalení oproti předchozím Paveway II/III představuje duální systém navádění. Spočívá v kombinaci GPS/INS (Inerciální navigační systém) a laserového navedení. V závislosti na konkrétních podmínkách může pilot na navedení použít buď jeden z těchto systémů nebo oba současně.

Operační nasazení
Paveway IV byla zařazena do výzbroje RAF v roce 2008 a ještě v témže roce byla bojové nasazení v Afghánistánu na letadlech Tornado GR4. V roce 2011 použili Britové tuto munici v Libyi během operace Ellamy. Formace britských stíhaček bombardovaly strategické budovy libyjské vlády a obrněnou techniku jednotek Muammara Kaddáfího. V září 2014 použila britská Tornáda pumy Paveway IV k bombardování těžkého dělostřelectva Islámského státu v severozápadním Iráku. Pozice Islámského státu v Sýrii byly bombardovány pumami Paveway IV prostřednictvím britských Eurofighter Typhoon.

Uživatelé

Royal Air Force

Královské letectvo Saúdské Arábie

Reference

Letecké pumy

redpajama_set_name: RedPajamaWikipedia


text:
Q: Reverse a dynamic array I have 'button' like this
<span data-id="dr21" data-minheight="100" data-maxheight="200" data-minwidth="20" data-maxwidth="50"  class="customsizebutton">(edit size)/span>

and script like this
<script>
$('.customsizebutton').click(function ()
{
var id = $(this).data('id');
var minHeight = $(this).data('minheight');
var maxHeight = $(this).data('maxheight');
var minWidth = $(this).data('minwidth');
var maxWidth = $(this).data('maxwidth');
var arrayH = [];
var arrayW = [];
for (var i = minHeight; i <= maxHeight-1; i++) {
arrayH.push(i);
}
for (var i = minWidth; i <= maxWidth-1; i++) {
arrayW.push(i);
}

var selectListH = document.getElementById("h-"+id);
for (var i = 0; i < arrayH.length; i++) {
var option = document.createElement("option");
 option.text = arrayH[i];
selectListH.appendChild(option);
}

var selectListW = document.getElementById("w-"+id);

for (var i = 0; i < arrayW.length; i++) {
var option = document.createElement("option");
 option.text = arrayW[i];
selectListW.appendChild(option);
}})
</script>

I am trying to fill the two dropdowns with
<option>200</option>
<option>199</option>...
<option>101</option>
<option>100</option>

<option>50</option>
<option>49</option>...
<option>21</option>
<option>20</option>

It currently fills the dropdowns the opposite direction (low to high). I'm new to this and trial and error has got me this far.
Thanks

A: Just populate the arrays in reverse order.
for (var i = maxHeight-1; i >= minHeight; i--) {
arrayH.push(i);
}
for (var i = maxWidth-1; i >= minWidth; i--) {
arrayW.push(i);
}

A: If you merely need to populate your dropdowns in reverse order, you can just iterate them in reverse, like so:
for (var i = arrayH.length - 1; i >= 0; i--) {
var option = document.createElement("option");
 option.text = arrayH[i];
selectListH.appendChild(option);
}

If you want to actually reverse the items in the array, as the title of your question denotes, that's even easier, with the Array.reverse function:
arrayH = arrayH.reverse();

If you're new, I recommend reviewing the JavaScript documentation over at Mozilla.


text:
Jedox announces U.S. expansion with new office in Seattle
Boston, February 4th, 2020 — Jedox, a leading global provider of cloud-based enterprise performance management software, has announced their expansion in the United States with the official opening of their new office in Seattle, Washington. The new office in Seattle answers the growing demand from organizations for a highly flexible EPM solution and strengthens the Jedox U.S. presence as the company continues to experience significant growth in the region.
As more organizations recognize the impact that Digital Transformation is having not just on the finance team but across numerous business functions, it is imperative that they are empowered with best-in-class solutions to meet these challenges.
"We are delighted to start this year with the announcement of our new U.S. office in Seattle," said Florian Winterstein, Jedox CEO. "This expansion is in close proximity to some of the world's largest and most established companies in the tech industry and allows us to continue building on our relationships and alliances there and deepen our commitment to helping organizations of all sizes improve their performance and competitive edge." Winterstein added.
The Seattle office joins the rest of the Jedox global offices in Singapore, Melbourne, Sydney, Paris, and the global headquarters in Germany. The expansion is in line with the global growth strategy and focus on continued development of the North American market.
The Jedox America President, Dr. Liran Edelist, commented "Seattle was the perfect choice for our expanded presence in the USA. We are very happy to be able to further extend our offerings for customers in the execution of their FP&A Digital Transformation roadmap with an extraordinarily flexible and user-friendly EPM solution."
Contact details for the new Seattle office can be found here
By Jedox|February 5th, 2020|
About the Author: Jedox
Jedox simplifies planning, analysis, and reporting with one unified and cloud-based software suite. Jedox empowers decision makers and business users across all departments and helps them work smarter, streamline business collaboration, and make insight-based decisions with confidence. Already 2,500 organizations in 140 countries are using Jedox for real-time planning on the web, the cloud, and on any device. Jedox is a leading Business Intelligence and Enterprise Performance Management solutions provider, available worldwide with offices in four continents and over 250 certified business partners.
Email: press@jedox.com
Phone: +49 (761) 15147 – 0
Stay up to date with the latest from Jedox and subscribe today.


text:
Marguerite Beaufort ( – ) est la fille de Jean Beaufort et de Marguerite Beauchamp (morte en 1482) et la nièce d'Edmond Beaufort, l'un des derniers commandants anglais de la guerre de Cent Ans. Elle est la mère du futur Henri VII d'Angleterre, son unique enfant.

Biographie

Premier mariage
Son père Jean Beaufort meurt dès 1444. Marguerite hérite de ses terres et biens, dont la garde sont cependant confiés à William de la Pole, duc de Suffolk, un des conseillers du roi Henri VI. En , alors qu'elle est encore une enfant, elle est mariée à John de la Pole, fils de Suffolk. Suffolk, accusé de trahison par ses adversaires, est banni pour cinq ans mais son bateau l'emmenant en France est intercepté par une bande de soldats mécontents appartenant au duc d'Exeter qui le condamnent à mort et le décapitent le . Le mariage de Marguerite et John est annulé en 1453. Dans son testament fait en 1472, Marguerite ne reconnaît pas cette union et cite Edmond Tudor comme son premier mari.

Deuxième mariage
Henri VI confie en  Marguerite à son demi-frère, Edmond Tudor, comte de Richmond. Elle l'épouse à 12 ans le . Edmond, partisan de la Maison de Lancastre, est emprisonné par les yorkistes en août 1456 dans la prison de Carmarthen, au pays de Galles, où la peste l'emporte le  suivant. Son frère Jasper Tudor, comte de Pembroke, prend en charge sa belle-sœur Marguerite Beaufort, alors enceinte à 13 ans d'Henri Tudor (futur Henri VII), lequel naît le  au château de Pembroke. Cette maternité précoce, même selon les standards médiévaux à l'époque, rend l'accouchement si difficile qu'il manque de faire mourir la mère et son enfant à naître et rendra irrémédiablement Marguerite stérile pour ses remariages ultérieurs selon beaucoup d'historiens.

Troisième mariage
Le , Marguerite épouse Henry Stafford, deuxième fils du duc de Buckingham. C'est un fervent défenseur de la Maison de Lancastre. Cependant, lorsque Édouard IV, chef de la Maison d'York, devient roi en , Stafford est pardonné par le roi. Marguerite vit avec son époux tandis que son fils est confié à William Herbert. Henri vit chez Herbert jusqu'à l'exécution de ce dernier le  dans la confusion de la bataille de Losecoat Field par Richard Neville, comte de Warwick, en rébellion ouverte contre le roi Édouard IV. Warwick renverse Édouard IV le  et restaure Henri VI. Édouard IV débarque en Angleterre le  et défait Warwick à la bataille de Barnet le . Étonnamment, Stafford se bat aux côtés des yorkistes. Il est grièvement blessé et meurt de ses blessures le . Henri Tudor, alors âgé de 14 ans, s'exile en France pour échapper aux représailles des yorkistes.

Quatrième mariage et reine de Man
En , Marguerite épouse Thomas Stanley qui, durant la Guerre des Deux-Roses, a pris parti parfois pour les Lancastre parfois pour les York. Elle revient à la cour d'Édouard IV et est brièvement dame d'honneur de la reine Élisabeth Woodville. Son mari est emprisonné en  par Richard III lorsque ce dernier s'empare du pouvoir mais il est rapidement libéré.

En , Marguerite soutient une rébellion contre Richard menée par le duc de Buckingham avec les partisans yorkistes du défunt Édouard IV. Buckingham échoue et est exécuté. Marguerite est assignée à résidence, en son château, sur ordre de Richard. Son époux est chargé d'assurer sa surveillance.

La mère du roi
En , lorsque Henri Tudor débarque sur les côtes d'Angleterre pour livrer bataille à Richard III, Marguerite Beaufort persuade Thomas Stanley de trahir Richard III pour soutenir son fils, Henri Tudor. À l'issue de la bataille de Bosworth, Stanley prend la couronne de Richard III pour la placer sur la tête de Henri Tudor, qui est alors proclamé roi d'Angleterre sous le nom d'Henri VII.

Stanley et Marguerite sont peu après nommés comte et comtesse de Derby. Durant le règne de son fils, Marguerite Beaufort ne s'est pas mêlée de politique et a joué un rôle plutôt discret. Elle est titrée Ma Lady la Mère du Roi.

Elle fonde deux collèges à Cambridge : le Christ's College en 1505 et le St John's College, achevé après sa mort en 1511.

Décédée en , deux mois après son fils, elle est enterrée près de lui à l'abbaye de Westminster.

Ascendance

Notes et références

Liens externes

Personnalité anglaise de la guerre de Cent Ans
Margaret
Personnalité de la guerre des Deux-Roses
Naissance en mai 1443
Décès en juin 1509
Décès à 66 ans
Personnalité inhumée à l'abbaye de Westminster
Dame de la Jarretière
Comtesse de Richmond
Comtesse de Derby
Maison Tudor


Home > Dispensing and Supply > How are your prescriptions processed?
Since the introduction of CIP, PSNC's auditing function (see this page for more details) has helped to identify some processing issues which had caused errors in payment for some prescription items. Error correction and system improvement work is ongoing, and both PSNC and NHSBSA are continuing to scrutinise the system closely.
NHSBSA's pricing system uses high-speed scanning equipment and Intelligent Character Recognition (ICR) software to support the capture of printed information from prescription forms. This is supplemented by the information input manually by NHSBSA's operators. Once information is captured, it is processed by the 'rules engine' to determine the payment due to contractors.
A summary of the key steps in the pricing process are outlined below. A diagram of this process can be downloaded here.
Prescription bundles received by NHSBSA must first be prepared for the scanning process which can be hindered by the way prescriptions have been submitted.
For information on how to properly sort your prescription bundle prior to submission please see our Sorting Your Prescriptions Prior to Submission page.
Once a prescription bundle is received, NHSBSA staff must make sure all clips, staples and sticky labels have been removed as they can jam or damage the scanning equipment. The information that has been entered onto the FP34c submission document is input alongside the scanned images and this is used to calculate the pharmacy's advance payment; therefore it is crucial that this has been completed accurately.
For more information/guidance on how to complete the submission document correctly, please see our Completing Your FP34c Submission Document & Dispatching Your Prescription Bundle page.
The scanning system is only used to support the capture of data from the prescription, for example the prescriber ID, prescription form type, exemption status and details of the prescribed items. If the scanning process cannot determine this information with confidence, for example if the prescription is handwritten, then the prescription will be referred to a Type 1 Exception Handler who will enter the prescription details manually.
At this stage if the system flags that a prescription may have been submitted in the incorrect charge group, it will be referred to a Type 1 Exception Handler for verification of whether the form was in fact submitted incorrectly or not. If it was submitted incorrectly then it will be switched. No forms are switched automatically by the system; they are only switched once verified by a trained member of staff.
Further guidance on switching is available on our Prescription Switching page.
Prescriptions which cannot be processed automatically by the system will be sent to an operator who will manually capture the relevant information required to price the prescription.
Items with prescriber handwritten amendments.
At this stage, items which still cannot be priced due to a lack of information must be referred back to the contractor for clarification. Payment will only be delayed for the item for which the clarification is required, and not for any other items which appear on the same prescription form. For more information on returned prescriptions and how to prevent these being returned please see our Prescription Returns page.
Once the data on the prescription forms has been confirmed, the information will be processed automatically via the 'rules engine'. This system will automatically apply the Drug Tariff rules for the month for which the prescriptions were submitted.
The total payment due for items dispensed will be calculated from the automatically captured data and the manually captured data. Any adjustments are made and the contractor's final payment is calculated.


SYSTEM BUILDERS ROUTINELY TEST their machines for speed and reliability, both to collect superlatives (fastest, coolest, quietest, and so on) that can be used in advertising and to reduce the chances that the PCs they send to customers will get sent right back. However, no two builders seem to use the same tests or get identical results using similar hardware.
Mike Beuligmann, president of St. Louis-based eCollegePC.com, feels the same way. Both companies, in fact, spend quite a bit of time on testing. And both say the more time the better.
Beuligmann has a list of favorite software tools for assessing computers. "We start with [Memtest86+] to test the memory and then run Prime95 with Real Temp to test the CPU and memory," he says. "Then we run 3DMark or UNIGINE Heaven 3D to test the video performance and the overall system." The complete process takes 24 to 72 hours, depending on the build, and according to Beuligmann is highly effective at verifying system quality and helping his company maintain high customer satisfaction ratings.
Velocity Micro's favored tools include Geekbench or PCMark to test the complete system, as well as CrystalDiskMark, 3DMark, UNIGINE Heaven, Intel Extreme Tuning Utility (XTU), and Cinebench for individual components. Since Covington prefers Samsung SSDs, his team relies on Samsung Magician for health and performance checks. The company also employs a custom application to run cores at 100 percent utilization overnight and takes care to ensure that the peripherals it uses, such as monitors and keyboards, all work well with its PCs.
While some companies see variations in test results between systems, Beuligmann rarely experiences that issue. "We use only high-end components on our builds so that may be why our results are consistent," he notes.
According to Covington, one reason test results tend to vary so widely is that vendors check the things that matter most to them. Workstations? Prove that the processors can handle the customer's workloads without overheating and failing. Gaming boxes? Give graphics a workout and measure screen refresh rates and latency. General office machines? Test boot time, network speed, built-in Wi-Fi consistency, and other factors.
One thing Covington has discovered is that minute differences in hardware, even between identical SKUs, can make a big difference in terms of reliability. The quality of the silicon used, minor fluctuations in how much power the device draws, and even driver optimization affect performance and therefore test results. That's one reason many system builders like extended burn-in times.
That persistence, along with patience, will ultimately pay off in the form of higher quality, happier customers, and a healthier balance sheet.


Of all the different Mexican Gold Pesos that the Casa de Moneda de México minted in the past, only the Hidalgo Gold Pesos were issued in multiple sizes. The coins that mostly depict a portrait of the pastor Don Miguel Hidalgo y Costilla on their obverse side exist in the denominations of 10 Peso, 5 Peso (1/2 Hidalgo), 2.5 Peso (1/4 Hidalgo) and 2 Peso (1/5 Hidalgo). The 2 Peso gold coin is an exception in that it displays a harvest wreath instead. Mexico's official coat of arms that shows an eagle perched on top of a cactus while holding a snake appears on the reverse side of all sizes of the Mexican Gold Hidalgo.
The four smallest Mexican Peso gold coins are composed of 90% gold and 10% copper just like the larger Mexican 50 Peso gold coins and Mexican 20 Peso gold coins. Mintage numbers as well as mintage periods differ significantly for the four different Mexican Hidalgo gold coins.
As a coin type, these Gold Peso coins aren't rare gold coins. The mintage numbers of the 2 ½ Peso gold coins were far lower than those of the other three denominations though. If you decide to buy gold in the form of these Mexican gold coins, you should know that all four coin denominations were heavily restruck in later years! American buyers that are investing in gold for their retirement should take note that all versions of the Mexican Gold Hidalgo coin are not eligible for inclusion in Individual Retirement Accounts (IRA's) since they are classified as collectible gold coins by the IRS.
The obverse side of the three largest Hidalgo Gold Pesos (10 Peso, 5 Peso and 2.5 Peso) bears the image of the pastor Don Miguel Hidalgo y Costilla, the Mexican "Father of the Nation" who started the revolution that escalated to the Mexican War of Independence on the 16th of September 1810. Hidalgo died as a martyr in front of an execution squad shortly after the revolution began. The 10 Peso gold coin ("Diez Pesos") and 5 Peso gold coin ("Cinco Pesos") has the denomination, year of mintage and mint mark M engraved along the coin's edge. The 2.5 Peso gold coin ("Dos Y Medio Pesos") doesn't contain a mint mark though.
The obverse design of the 2 Peso gold coins is different in that it only depicts a harvest wreath along with the coin's denomination ("Dos Pesos"), the year of mintage on top and the mint mark of the mint in Mexico City at the bottom.
The Mexican Coat of Arms is depicted on the reverse side of the coins. It shows an eagle perched upon a cactus that is holding a serpent in its powerful beak and talons. The inscription "Estados Unidos Mexicanos" appears above the image of the eagle.
The edge of the 10 Peso gold coins and 5 Peso gold coins is lettered with the words INDEPENDENCIA Y LIBERTAD (Independence and Freedom).
Mexico carried out a monetary reform in 1905 that resulted in the introduction of many new coins by the Casa de Moneda de México in the years that followed. The 10 and 5 Mexican Gold Pesos were already introduced in 1905. The 2.5 and 2 Gold Peso coin followed much later in 1918 and 1919.
All four denominations of the Mexican Gold Hidalgo were heavily restruck. The 10 Peso coin had 954,983 pieces restruck between 1961 and 1972. These restrikes bear the date 1959 which makes it very hard to impossible to distinguish them from the original 1959 coins. Matte restrikes of the 10 Peso Hidalgo gold coin were issued in 1996.
The 5 Peso (1,767,645 restrikes), 2.5 Peso (5,025,087 restrikes) and 2 Peso coins (4,590,493 restrikes) were all restruck between 1951 and 1972. The 5 Peso restrikes bear the date 1955 but both the 2.5 Peso and 2 Peso restrikes bear the date 1945. Additionally, 89,000 matte restrikes of the 5 Peso coin were made between 2000 and 2009.
More than 8.2 million 10 Peso gold coins were minted between 1905 and 1959. Annual mintage numbers varied from only 12,000 coins in 1920 to almost 3 million pieces in 1906.
More than 9.3 million 5 Peso gold coins were minted between 1905 and 1955. The lowest mintage year was 1905 with 18,000 pieces which was followed by the highest mintage year in 1906 when more than 4.6 million coins were minted.
More than 3.7 million 2 1/2 Peso gold coins were minted between 1918 and 1948. Only 20,000 pieces were struck in 1944 and only 24,000 in 1947. The highest mintage year was 1918 with more than 1.7 million coins.
More than 6.3 million 2 Peso gold coins were minted between 1919 and 1948. Only 10,000 pieces were minted in 1944 whereas close to 4.3 million coins had been minted in 1920. The fate of the 45,000 coins that were supposedly minted in 1948 is unknown since none are known to exist. Any 1948 issues that are available on the market can be presumed to be counterfeit.


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More clearly, My Brute is a mini fighting game in which you must battle other brutes (players) scattered throughout the world. In reality, we do not directly control its raw because once the game started, the fighting takes place automatically. Nevertheless, one can follow their evolution as gain experience, skills and unlock new weapons.
Unfortunately your raw skills can not be determined at the creation, you can simply customize the look, and after you will be able to climb in levels, in order to gain new skills, weapons and even pets (Wolf, panther, tiger, etc.). Rule: you will receive six fights per day and gross.
Unlock and personalise up to 9 brutes.
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text:
Indonesia set to ink trade deal with Chile by year-end
President Widodo embraces openness, shifting country away from protectionism
KAZUKI KAGAYA, Nikkei senior staff writer December 08, 2017 15:45 JST
Chilean President Michelle Bachelet chats with her Indonesian counterpart, Joko Widodo, during her visit to the presidential palace in Jakarta in May. © Reuters
TOKYO -- Indonesia plans to sign a free trade agreement with Chile by the end of this year, Indonesian Trade Minister Enggartiasto Lukita has said.
Jakarta is also holding talks on free trade pacts with Australia, the European Union, the European Free Trade Association and Iran, as it tries to lift economic growth by finding new export markets.
EU asking for 'trade war' with palm oil curbs: Indonesian minister
Malaysia and Indonesia mull free trade zone in Borneo at annual summit
Among Southeast Asian nations, Indonesia is said to be at a disadvantage when it comes to exports because it has few free trade deals with other countries.
Lukita, who spoke with the Nikkei Asian Review when he visited Japan in late November, said he would visit Santiago, Chile, to sign the agreement after attending the ministerial meeting of the World Trade Organization to be held in Buenos Aires, Argentina from Sunday to Wednesday.
Indonesian Trade Minister Enggartiasto Lukita (Photo by Keiichiro Sato)
Although details on the pact have not been disclosed, it is a comprehensive economic partnership agreement and expected to include the scrapping or lowering of tariffs and nontariff barriers on trade in goods and measures to facilitate investment.
Indonesian Ambassador to Chile Gonzalo Mendoza Negri was quoted in an Indonesian news report in September as saying the two countries need to cooperate in mining and geothermal energy.
Both Indonesia and Chile are members of the Asia-Pacific Economic Cooperation forum. Trade between the two countries totaled $230 million in 2016, according to the International Trade Center. It seems that they can easily reach a deal, given there are no major trade disputes between them.
Indonesia is also negotiating a free trade agreement with Australia. Lukita said the two countries would "finalize" a deal by the end of the year. "The final draft will be realized next year," he added, suggesting they will work out details early in 2018.
Indonesia has also been holding talks with the EU and the EFTA, which comprises four non-EU countries: Iceland, Norway, Switzerland and Lichtenstein. In addition, it is accelerating talks with Iran over a preferential trading area.
Although Indonesia is pushing to conclude free trade accords, it has a number of disputes with prospective partners that may hamper its efforts. Australia accuses it of exporting copier paper to Australia at unfairly low prices, for example.
The U.S. has slapped anti-dumping duties on paper products from Indonesia. Although Jakarta filed a complaint against the U.S. move with the WTO, a dispute-resolution panel ruled against it on Wednesday.
The European Parliament has also questioned the clearing of forested land for production of palm oil in Indonesia, and the EU is weighing restrictions on imports of the product.
Indonesia has traditionally been cool to free trade deals, or dragged its feet with parliamentary ratification, for fear of hurting domestic industry. It has concluded fewer trade accords than its neighbors such as Singapore, Thailand and Vietnam. An economic partnership agreement with Japan is one of the few deals it has signed.
But President Joko Widodo, who took office in October 2014, has been more positive about international trade. Indonesia is striving for an early conclusion to the 16-nation Regional Comprehensive Economic Partnership, which includes Japan, China and India. It is also working on deals with the nine other members of the Association of Southeast Asian Nations.
According to ITC data, in 2016, Indonesia's exports fell 4% on the year to $144.49 billion, while imports declined 5% to $135.65 billion. The country's current-account deficit reached $16.90 billion last year.
Indonesia, like other developing countries, tends to increase imports when its economy is growing rapidly, with investment from abroad rising as domestic manufacturing capacity is strained. Unless Indonesia can create an environment favorable for exports through trade agreements with other countries, its currency, the rupiah, will come under pressure as its trade and current-account deficits rise.
At a time when U.S. financial authorities are moving toward raising interest rates, Indonesia is looking to trade both to stimulate its economy and to protect its currency.
Bank Indonesia cuts rate in anticipation of Fed easing
Credit cards fall behind in Asia's race to go cashless


text:
\section{Introduction}
WD~J2356$-$209\footnote{Also known as WD~2354$-$211 in the electronic version of
of the Catalog of Spectroscopically Identified White Dwarfs \citep{mccook1999catalog}},
was discovered by \cite{oppenheimer2001direct} as part of their search
for cool white dwarfs in the galactic halo. Since its spectrum shows a broad asymmetric
feature around 6000{\,\AA}, it was described as having a "bizarre spectrum,
incomparable to any other known object".

Using only $BRI$ photometry, \cite{bergeron2003critical} attempted the first atmospheric
parameter determination of WD~J2356$-$209. It was found that it must have an effective
temperature of the order of $4000\,{\rm K}$: the best photometric solution was at
$T_{\rm eff}=3400\,{\rm K}$ if a hydrogen-rich atmosphere was assumed and
at $T_{\rm eff}=4610\,{\rm K}$ in the case of a helium-rich composition.
Note that because of the absence of Balmer lines at such low temperatures, the atmospheric
composition of this object remained unknown.

Shortly after, \cite{salim2004cool} reobserved WD J2356$-$209 and confirmed the measurements
of \cite{oppenheimer2001direct}. In particular, in a color-color diagram,
it appears as a strong outlier
with an excessively blue $B-V$ and an extremely red $V-I$. \cite{salim2004cool} suggested
that these peculiar colors may be the result of a very broad \ion{Na}{1} D doublet, implying that
WD~J2356$-$209 is a metal-polluted white dwarf (i.e., a DZ star).

Then, \cite{bergeron2005interpretation} obtained new photometric observations of
WD~J2356$-$209 in the $BVRI$ and $JH$ bands. They picked up the interpretation proposed
by \cite{salim2004cool} and analyzed WD~J2356$-$209 with atmosphere models that included Na.
Their solution ($T_{\rm eff}=4790\,{\rm K}$ and $\log\,{\rm Na/He}=-5$)
yields a satisfactory fit both to their photometric measurements and
to the spectrum of \cite{oppenheimer2001direct} in the 5000--9000{\,\AA} region.
However, in the absence of any spectrum below 5000{\,\AA} they could not detect any
other metal than Na, and thus Na and He were the only atomic species included in their
atmosphere model. In retrospect, this was an unrealistic assumption.
With the discovery of dozens of circumstellar debris discs around metal-polluted white dwarfs
\citep[e.g.,][]{zuckerman1987excess,gansicke2006gaseous,farihi2009infrared,melis2010echoes,rocchetto2015frequency}
and the detection of planetary transits in the light curve of WD~1145+017
\citep{vanderburg2015disintegrating,gansicke2016high,croll2017multiwavelength}
it is now clear that the presence of heavy elements in white dwarfs is the
consequence of the accretion of tidally disrupted rocky bodies
\citep{jura2003tidally,farihi2010rocky,jura2014extrasolar}.
Therefore, all elements representative of the composition of rocky planetesimals
should be included in DZ atmosphere models.

Moreover, the analysis of \cite{bergeron2005interpretation}
was based on models that did not take into account the nonideal high-density effects that are known to
arise under the physical conditions met in the atmospheres of cool white dwarfs. In particular,
their models relied on the ideal gas law, which is inappropriate for the high pressures of cool white dwarfs
\citep[e.g.,][]{saumon1995equation,becker2014ab};
nonideal effects affecting the chemical equilibrium \citep{kowalski2007equation,blouin2018model} were neglected;
and simple Lorentzian line profiles, which poorly reproduce the spectral lines observed in cool DZ
white dwarfs \citep{allard2016asymmetry,allard2018line,hollands2017cool}, were assumed.

An independent analysis of WD~J2356$-$209 was performed by \cite{homeier2005,homeier2007}
using the PHOENIX general-purpose stellar atmosphere code \citep{phoenix1,phoenix2,phoenix3}
and the spectrum obtained by \cite{oppenheimer2001direct}.
The first results identified an apparent overabundance of Na relative to Ca and suggested
that WD~J2356$-$209 has a hydrogen-rich atmosphere \citep{homeier2005}. An important limitation
of this first analysis was that line profiles implemented in their atmosphere models
were limited to perturber densities not exceeding $10^{19}\,{\rm cm}^{-3}$
\citep{allard2003new}, which is about three orders of magnitude below the density
at the photosphere
of a $T_{\rm eff}=4000\,{\rm K}$ helium-rich DZ white dwarf \citep{blouin2018model}.
In a second analysis
\citep{homeier2007}, improved line profiles appropriate for larger densities were employed and
a helium-rich composition was favored. \cite{homeier2005,homeier2007} were also
the first to point out that metal hydrides (namely, MgH and CaH) should form under the
conditions encountered in the atmosphere of WD~J2356$-$209. However,
these preliminary analyses were exploratory in nature and no quantitative fit to
the spectroscopic and photometric data was attempted. Furthermore, as in
\cite{bergeron2005interpretation}, their models did not include the nonideal effects that
are known to affect the chemical equilibrium and the equation of state.

In this paper, the third of a series, we present the most detailed analysis to
date of WD~J2356$-$209. Our models, which
include an accurate description of the high-pressure physics relevant to the
modeling of cool DZ stars (see \citealt{blouin2018model,blouin2018dzcia}, hereafter
Papers~I and II),
make it possible for the first time to obtain a
satisfactory fit to the photometric data and to the entire visible spectrum.
In Section \ref{sec:observations}, we present the observations on which
our analysis of WD~J2356$-$209 is based.
A few new improvements brought to our model atmosphere code
are detailed in Section \ref{sec:models}. Section \ref{sec:analysis} contains
our analysis of WD~J2356$-$209, where we find that the sodium to calcium ratio is the
highest ever encountered in a white dwarf photosphere.
Finally, Section \ref{sec:interpretation} provides a discussion on the origins of the peculiar
abundances measured in WD~J2356$-$209 and our conclusions are given in Section \ref{sec:conclusion}.

\section{Observations}
\label{sec:observations}
Our analysis of WD~J2356$-$209 makes use of $BVRI$ and $JH$ photometry from
\cite{bergeron2005interpretation}, $grizy$ photometry from Pan-STARRS
\citep{chambers2016panstarrs} and the \textit{Gaia} DR2 parallax measurement
\citep{prusti2016gaia,brown2018gaia}. The parallax indicates that
WD~J2356$-$209 is located at a distance $D = (64.8 \pm 2.5)\,{\rm pc}$ from
the Earth, which is in good agreement with the estimation obtained by
\cite{salim2004cool} using color-magnitude relations ($74 \pm 34\,{\rm pc}$).

For the spectroscopy, we rely on data obtained
with LRIS \citep{oke1995keck} on Keck I
telescope on 2002 September 14.
A 300/5000 grating was used for both the
blue and the red spectra, together with a 1 arcsec slit, giving an
effective resolution of 10.3\,{\AA}. D560 dichroic was used to split the
beams, giving useful wavelength coverage of 5000$-$9000\,{\AA} on the red
side and 3500$-$5800\,{\AA} on the blue side. Each of the blue and red
spectra were obtained with a total exposure time of 45 minutes. Standard
arc spectra were taken for wavelength calibration. Only one standard
star was available for flux calibration, while there were no suitable
observations for the removal of the telluric absorption. The
observations of the standard star may have been affected by detector
non-linearity. Therefore, we correct the flux calibration by scaling the
spectrum so that the photometry extracted from the joined blue/red
spectrum agrees with the broad-band photometry.
As shown in Figure \ref{fig:2356obs}, the scaled LRIS spectrum
agrees very well with the low-resolution shallow spectrum of
\cite{oppenheimer2001direct} in the region where they overlap ($>5000\,${\AA}).

\begin{figure}
    \includegraphics[width=\columnwidth]{f1.pdf}
    \caption{Observed spectra and photometry of WD~J2356$-$209. The spectrum of
      \cite{oppenheimer2001direct} is in gray and the Keck LRIS
      spectrum is in blue. Note that the LRIS spectrum was scaled so
      that the predicted photometry (blue circles) match the observed
      photometry (black error bars).}
  \label{fig:2356obs}
\end{figure}

\section{Atmosphere models}
\label{sec:models}
The atmosphere models used in this work are described at length in Paper I.
Our models are uniquely suited for the analysis of such a very cool DZ star, since they are
the only ones to include both a state-of-the-art description of the
ionization equilibrium of heavy elements (Paper I) and unified line profiles
  \citep{allard1999effect} for the strong Na and Ca spectral lines that characterize
  the spectrum of WD~J2356$-$209.

Compared to the models used in Papers I and II, two changes were made to our code.
First, we have improved our collisional profiles of the resonance
line of neutral calcium perturbed by helium using the ab initio Ca$-$He potential energies of
M. Kro{\'s}nicki reported in \cite{hernando2008absorption}. It is a significant improvement in
the description of Ca$-$He singlet potential energies, but only at close range
(i.e., only for radiator-perturber separations of $\approx 3.5$ to 11{\,\AA}).
To predict the impact core shift and width, the long-range part of the potential energies
needs to be accurately determined. Moreover, our approach requires prior knowledge of the
variation of the radiative dipole moments with atom-atom separation for each molecular state.
As this variation is unknown at present, the dipole moments were assumed to remain constant
throughout the collision. In order to obtain more
accurate line profiles, intensive ab initio calculations are being performed to obtain both
the ground and first excited potential energy curves (PECs) and the transition dipole
moments for the Ca$-$He system (N.~F. Allard et al., in preparation).

The second change made to our atmosphere model code was to add the opacity due
to the rovibrational transitions of the MgH and CaH molecules.
The MgH opacities are computed using the linelists of \cite{GharibNezhad2013einstein}
for the the X$^2\Sigma^+ \rightarrow$ A$^2\Pi$ and X$^2\Sigma^+ \rightarrow$ B$'^2\Sigma^+$
transitions, which are available on the ExoMol website\footnote{\url{http://exomol.com}}
\citep{tennyson2012exomol,tennyson2016exomol}.
For CaH, the X$^2\Sigma^+ \rightarrow$ A$^2\Pi$ and X$^2\Sigma^+ \rightarrow$ B$^2\Sigma^+$
transitions are computed
using the Kurucz linelists\footnote{\url{http://kurucz.harvard.edu}}, which
rely on molecular data from \cite{weck2003vibration} and \cite{shayesteh2013fourier}.

\section{Analysis of WD~J2356$-$209}
\label{sec:analysis}
We rely on the $BVRIJH$ and $grizy$ photometry of WD~J2356$-$209 to find its effective
temperature, surface gravity and H/He abundance ratio. More specifically, the solid angle
$\pi \left( R/D \right)^2$ and $T_{\rm eff}$ are found by fitting the model fluxes to the
spectral energy distribution. Since the distance $D$ is already known from the \textit{Gaia} parallax, we
can obtain the radius $R$ from the solid angle. The mass of the white dwarf (and the corresponding
surface gravity) are then found using the evolutionary models of \cite{fontaine2001potential}
with C/O cores, $\log \left( M_{\rm He} / M_{\star} \right) = -2$ and
$\log \left( M_{\rm H} / M_{\star} \right) = -10$, which are representative of
helium-atmosphere white dwarfs.
The H/He abundance ratio is inferred from the infrared photometric measurements, which
are affected by the presence of H$_2-$He collision-induced absorption
\citep[CIA,][]{jorgensen2000atmospheres,blouin2017cia}.
Once a photometric solution is found, we use
the spectroscopic data to constrain the abundances of Na, Ca, Fe and Mg.
In particular, the \ion{Na}{1} D doublet is used to derive the Na/He ratio, the \ion{Ca}{1} 4226{\,\AA}
and \ion{Ca}{2} H \& K lines for Ca/He, \ion{Fe}{1} and \ion{Fe}{2} lines in the 3600--3800{\,\AA}
region for Fe/He, and the MgH rovibrational bands between 5000 and 5300{\,\AA}
for Mg/He. Once the heavy element abundance ratios are found, the whole fitting procedure --
including the photometric fit -- is repeated until internal consistency is reached.

Figure \ref{fig:2356fit} compares our best solution to the photometric and spectroscopic data.
Except for the core of the \ion{Na}{1} D doublet and an unknown feature near 4500{\,\AA},
our fit is in excellent agreement with the observations across all wavelengths. In particular,
our spectroscopic fit closely matches the Fe lines at small wavelengths, the
\ion{Ca}{2} H \& K and \ion{Ca}{1} 4226{\,\AA} lines, the blue and red wings of the
\ion{Na}{1} D doublet, and the flux depletion between 5000 and 5500{\,\AA}.
Note that due to strong telluric absorption we could not use the \ion{Na}{1}
  doublet at 8200{\,\AA} to validate the sodium abundance inferred from the \ion{Na}{1} D doublet.
Regarding the photometric fit, we found that a mix H/He atmosphere has to be assumed to produce the
H$_2-$He CIA that is required to properly match the $J$ and $H$ bands.

\begin{figure}
    \includegraphics[width=\columnwidth]{f2.pdf}
    \caption{Our best solution for WD~J2356$-$209. The top panel shows our fit (in red)
    to the visible spectrum (in black) and the bottom panel shows our photometric
    fit to the $BVRI$, $JH$ and $grizy$ bands (the photometric observations are represented
    by the error bars). The dashed spectrum in the bottom panel
    was computed from our best-fitting model, but
    without including H$_2-$He CIA in the synthetic spectrum calculation.
    The strong absorption lines near 7600{\,\AA} are of telluric origin and were ignored
    in our analysis.}
  \label{fig:2356fit}
\end{figure}

The atmospheric parameters of WD~J2356$-$209 are given in Table \ref{tab:2356}.
Its very cool temperature of $T_{\rm eff}=4040 \pm 110\,{\rm K}$ makes
it -- to our knowledge -- the oldest known DZ star, with a cooling age of
$8.0 \pm 0.8\,{\rm Gyr}$.\footnote{Note that \cite{giammichele2012know}
    found a greater cooling age ($8.5\,{\rm Gyr}$) for WD~2251$-$070.
    However, their analysis
    was based on a model atmosphere code \citep{dufour2007spectral} that did not include a detailed
    description of the high-density effects arising at the photosphere of such a cool
    object. Our reanalysis of WD~2251$-$070 (Section \ref{sec:4500}) suggests
    that it has an effective temperature $T_{\rm eff}=4050 \pm 60\,{\rm K}$ and
    a surface gravity $\log g=7.94 \pm 0.04$, which corresponds to a cooling age
    of $7.5 \pm 0.5\,{\rm Gyr}$.}

Table \ref{tab:2356} also lists the constraints on metal abundance
ratios in the atmosphere of WD~J2356$-$209. Apart from the sodium abundance,
which is further discussed in Section \ref{sec:interpretation}, all abundances
are close to the average values measured in metal-polluted atmospheres.
In particular, in a ternary diagram of Ca, Mg and Fe abundances
\citep[e.g.,][Figure 2]{hollands2018cool}, WD~J2356$-$209 would be close to the bulk of DZ stars.
The constraints on Al, K, Ti, Cr, Mn and Ni,
for which no feature is observed in the spectrum of WD~J2356$-$209,
were found by raising their abundances up to the point where a spectral
line should be visible. Note that the constraint on the K/He ratio was found using
the spectrum of \cite{oppenheimer2001direct} instead of the LRIS spectrum, since the
latter shows strong telluric features near the \ion{K}{1} 7665/7699{\,\AA} lines
(see Figure \ref{fig:2356obs}). The constraint on C/He was established using the C$_2$
rovibrational bands instead of the atomic carbon lines, since the former require a smaller
carbon abundance before being visible in the spectrum. Finally, no firm constraints could be
found for the abundances of O and Si, since even the addition of a very large amount of
these elements does not result in any visible spectral lines. The limits for O/He and Si/He
given in Table \ref{tab:2356} are therefore lower-bound estimates of the maximum
abundance of these elements that is compatible with the spectroscopic observations of
WD~J2356$-$209.

\begin{deluxetable}{cc}
  \tablecaption{WD~J2356$-$209 atmospheric parameters \label{tab:2356}}
  \tablehead{\colhead{\hspace{0.7cm}Parameter}\hspace{0.7cm} &
    \colhead{\hspace{0.7cm}Value}\hspace{0.7cm}}
  \startdata
  $T_{\rm eff}$       & $\phn \phn \phd 4040 \pm 110\,{\rm K}$\\
  $\log g$            & $\phn \phd 7.98 \pm 0.07$\\
  $\log\,{\rm H/He}$\tablenotemark{a}  & $-1.5 \pm 0.2$\\
  $\log\,{\rm C/He}$  & $<-6.0$ \\
  $\log\,{\rm O/He}$  & $(<-4)$\tablenotemark{b}\phd\\
  $\log\,{\rm Na/He}$ & $-8.3 \pm 0.2$\\
  $\log\,{\rm Mg/He}$ & $-8.0 \pm 0.2$\\
  $\log\,{\rm Al/He}$ & $<-8.8$\\
  $\log\,{\rm Si/He}$ & $(<-6.8)$\\
  $\log\,{\rm K/He}$  & $<-10.0$\\
  $\log\,{\rm Ca/He}$ & $-9.3 \pm 0.1$\\
  $\log\,{\rm Ti/He}$ & $<-9.8$\\
  $\log\,{\rm Cr/He}$ & $<-9.9$\\
  $\log\,{\rm Mn/He}$ & $<-10.7$\\
  $\log\,{\rm Fe/He}$ & $-8.6 \pm 0.2$\\
  $\log\,{\rm Ni/He}$ & $<-8.0$
  \enddata
  \tablenotetext{a}{All abundances are reported as ratios of number densities}
  \tablenotetext{b}{The abundances in parentheses are not firm limits (see text)}
\end{deluxetable}

Our excellent fit to the wings of the broad Ca and Na spectral lines of WD~J2356$-$209 (Figure \ref{fig:2356fit})
was made possible
thanks to the improved lines profiles implemented in our models \citep{allard2014caii,allard2014nai}.
This good agreement
indicates that our model predicts the right physical conditions in the line-forming regions of the
atmosphere. In particular, it suggests that the total number density $n_{\rm tot}$ is accurate,
since it is the parameter that governs the broadening of the spectral lines.
At the photosphere of WD~J2356$-$209, the pressure is high enough ($\log P = 10.0$) that deviations
from the ideal gas law begin to be important (see Figure 4 of Paper I).
If the ideal gas law was assumed, $n_{\rm tot}$ would be 20\% higher and the line profiles
would be slightly broader (particularly the \ion{Na}{1} D doublet).
Note though that WD~J2356$-$209 cannot be used to validate our implementation of pressure
ionization, since its photospheric density ($\rho = 0.1\,{\rm g}\,{\rm cm}^{-3}$) is too small
to induce significant deviations from the ideal Saha equation \citep[][Paper I]{kowalski2007equation}.

\subsection{Collision-induced absorption}
Figure \ref{fig:cia} compares the H$_2-$He CIA profiles obtained by different authors
for physical conditions that are representative of the photosphere of WD~J2356$-$209. Differences
between the profiles imply that the H/He ratio derived from the photometry depends on the choice of
the CIA profiles implemented in our models. In particular, if the
profiles of \cite{jorgensen2000atmospheres} were assumed, a smaller hydrogen abundance
would be found. In fact, as already noted
in Paper II, the profiles of \cite{jorgensen2000atmospheres} predict a too strong
absorption in the $\approx 1.2-2\,\mu{\rm m}$ region, possibly because the potential energy and induced
dipole surfaces used to derive those profiles were computed with a smaller atomic orbital basis set.

\begin{figure}
    \includegraphics[width=\columnwidth]{f3.pdf}
    \caption{H$_2-$He CIA profiles at $4000\,{\rm K}$ and $n_{\rm He}=1.5 \times 10^{22}\,{\rm cm}^{-3}$,
      as computed by \citet[Equation 7]{blouin2017cia}, \cite{abel2012infrared} and \cite{jorgensen2000atmospheres}.
      The absorption profiles are divided by the number density of H$_2$ and He and are therefore
      constant with respect to density (with the exception of the \citeauthor{blouin2017cia} profile, which
      includes the effects of many-body collisions).}
  \label{fig:cia}
\end{figure}

Furthermore, Figure \ref{fig:cia} shows that significant differences between the profiles
of \cite{abel2012infrared} and \cite{blouin2017cia} appear above $2\,\mu{\rm m}$ (particularly
near the maximum of the fundamental band at $\approx 2.5\,\mu{\rm m}$). Those differences
are due to many-body collisions (which are only included in the profiles of \citeauthor{blouin2017cia})
that lead to an enhancement and a distortion of the absorption profile. The only photometric measurements
available beyond the $H$ band are those from the Wide-field Infrared Survey Explorer
\citep[WISE,][]{wright2010wide} for the 3.4 and 4.6\,$\mu$m bands. Our best fit is compatible with those
measurements, but their large uncertainties do not allow us to explicitly confirm that
the CIA is indeed enhanced by many-body effects.

\subsection{The Na$-$He satellite and the MgH bands}
The wide absorption feature in the blue wing of the \ion{Na}{1} D doublet proved particularly
challenging to model. \cite{allard2014nai} suggested that it could be the result of the
quasi-molecular satellite feature arising from the Na$-$He interaction. Our detailed analysis
reveals that it is only part of the explanation and that MgH rovibrational bands must be included
to fully explain this absorption feature. Figure \ref{fig:2356mgh} compares our best fit to the
5000--5500{\,\AA} absorption feature with and without the MgH bands. Clearly, the Na$-$He satellite
visible in the fit that omits the MgH bands (dashed line) is not sufficient to explain the whole
absorption feature and MgH absorption bands must be invoked.

\begin{figure}
    \includegraphics[width=\columnwidth]{f4.pdf}
    \caption{Comparison between the best solutions found when including (solid line) and when
    omitting (dashed line) the MgH bands in our models.}
  \label{fig:2356mgh}
\end{figure}

We emphasize that including MgH in our models is physically motivated.
Given the temperature of WD~J2356$-$209, its hydrogen
abundance (independently constrained from the H$_2-$He CIA) and the presence of magnesium
(which is given by a Mg/Ca ratio that is very close to the value expected for chondrite-type material),
MgH has to be present at the photosphere of WD~J2356$-$209. To our knowledge,
this is the first detection of MgH molecular features in a white dwarf. MgH bands
were proposed by \cite{dufour2006model} to explain the asymmetry of the \ion{Mg}{1} 5175{\,\AA} line
in G165$-$7, but it was later shown that improved line profiles -- beyond the impact
approximation -- are enough to explain this asymmetry \citep{allard2016asymmetry}.
Finally, note that for our derived atmospheric parameters CaH is not sufficiently abundant to produce
visible bands around 7000{\,\AA}.

\subsection{The unknown absorption feature near 4500\,\AA}
\label{sec:4500}
Our fit of WD~J2356$-$209 does not reproduce the small asymmetric absorption feature
near 4500{\,\AA} (Figure \ref{fig:2356mgh}). Technically, boosting the Ti/Ca ratio
by a factor of $\approx 10$ with respect to chondritic abundances allows the
\ion{Ti}{1} $a^5F - y^5F^{\circ}$ multiplet (centered
at 4535{\,\AA}) to be strong enough to reasonably match the absorption feature
near 4500{\,\AA}. However, another cool DZ star, WD~2251$-$070, offers good reasons to
be suspicious of this interpretation.

Indeed, WD~2251$-$070 also shows a strikingly similar absorption feature in that region
(Figure \ref{fig:2251comparaison}). Using photometric and spectroscopic data reported in
\cite{bergeron1997chemical} and \cite{dufour2007spectral}, we analyzed WD~2251$-$070 with
our cool DZ grid. Our preliminary fit yields $T_{\rm eff}=4050 \pm 60\,{\rm K}$,
$\log g = 7.94 \pm 0.04$, $\log\,{\rm H/He} <-4.5$, $\log\,{\rm Na/He} < -10.3$
and $\log\,{\rm Ca/He} = -10.0 \pm 0.1$ (an in-depth analysis of this object will
be presented in N.~F. Allard et al., in preparation).
Given the strong similarities between WD~2251$-$070 and WD~J2356$-$209 (i.e., same feature near 4500{\,\AA},
similar Ca abundances and virtually identical effective temperatures),
it is very likely that the origins of the
4500{\,\AA} absorption feature are the same for both objects.
If it is the case, then there is a good reason to reject Ti as the explanation for this feature.
Boosting the Ti ratio to produce a sufficiently strong
\ion{Ti}{1} $a^5F - y^5F^{\circ}$ multiplet also implies that
the similarly important $a^5F - y^5 G^{\circ}$ multiplet (centered around 5020{\,\AA})
should be visible. By adjusting the Mg abundance, our fit of WD~J2356$-$209 could accommodate
the additional opacity resulting from the \ion{Ti}{1} $a^5F - y^5 G^{\circ}$
multiplet. However, the spectrum of
WD~2251$-$070 clearly rules out the presence of any absorption feature around 5020{\,\AA}
and thus suggests that Ti cannot be the explanation of the 4500{\,\AA} absorption feature.

\begin{figure}
    \includegraphics[width=\columnwidth]{f5.pdf}
    \caption{Comparison of the spectrum of WD~J2356$-$209 to that of
      WD~2251$-$070. The data for WD~2251$-$070 is from
      \cite{bergeron1997chemical} and \cite{dufour2007spectral}.
      Note the resemblance between both spectra
      below 4600{\,\AA} and their strong dissimilarity at longer wavelengths.
    }
    \label{fig:2251comparaison}
\end{figure}

Still, since we rely on Lorentzian line profiles for
all Ti spectral lines, we need to be careful before completely ruling out Ti as the source of
the 4500{\,\AA} feature.
In principle, it is possible that accurate line profile calculations will show that the
$a^5F - y^5 G^{\circ}$ multiplet is flattened out under the density
conditions encountered at the photosphere of WD~2251$-$070 ($n_{\mathrm He} \approx 6 \times 10^{22}\,{\rm cm}^{-3}$).
However, there is a second argument against the Ti scenario. We constrained the Na abundance in
WD~2251$-$070 to $\log\,{\rm Na/He}<-10.3$, implying that it has a $\log\,{\rm Na/Ca}$ ratio smaller than $-0.3$.
This ratio is vastly different from the $\log\,{\rm Na/Ca}=1.0$ ratio found for WD~J2356$-$209 and we therefore
expect the abundance pattern of WD~2251$-$070 to be quite different from that of WD~J2356$-$209. In particular,
it would be surprising if WD~2251$-$070 and WD~J2356$-$209 had similar Ti/Ca ratios but
significantly different Na/Ca ratios. All things considered, it is unlikely that the feature
near 4500{\,\AA} is due to Ti.

Alternatively, since it is observed in two white dwarfs with similar Ca abundances,
it is tempting to explain the 4500{\,\AA} feature as being due to Ca.
In a dense helium medium, it turns out that the \ion{Ca}{2} H \& K profile
can show a quasi-molecular feature near 4500{\,\AA} \citep{allard2014caii}. However, for the physical
conditions in the atmosphere of WD~2251$-$070 and WD~J2356$-$209, this quasi-molecular line is
predicted to be too weak to explain the shape of the spectrum around 4500{\,\AA}. We are therefore unable
to identify the origin of this feature at the moment.

\section{How to explain the high sodium abundance?}
\label{sec:interpretation}
As it is well above the chondritic value of $\log\,{\rm Na/Ca}=0.0$ \citep{lodders2003solar},
the $\log\,{\rm Na/Ca}=1.0\pm0.2$ ratio measured in WD~J2356$-$209 is surprising and needs
to be explained. Note that this extreme abundance ratio is not only supported by our excellent fit
to the observations (Figure \ref{fig:2356fit}), but also by the direct comparison of
WD~J2356$-$209 to WD~2251$-$070. While both objects have a very similar calcium abundance and
a virtually identical effective temperature, their spectra are drastically different in the
region affected by the \ion{Na}{1} D doublet (as seen in Figure \ref{fig:2251comparaison}).

\subsection{Comparison to other sodium-rich stars}

WD~J2356$-$209 is not the only white dwarf to have a high Na/Ca abundance ratio.
A few objects with $\log\,{\rm Na/Ca}>0$ were identified by \cite{hollands2017cool}
and are shown in Figure \ref{fig:diffusion_evolution}.
However, because of the very noisy spectra of many of those objects,
the derived abundances are often highly uncertain. Using our own atmosphere model grid,
we performed a reanalysis of this sample and we found that, within the uncertainties,
most of those objects are compatible with a chondritic abundance ratio of $\log\,{\rm Na/Ca}=0$
(a detailed analysis will be presented in S.~Coutu et al., in preparation).
In fact, we found compelling evidence of a high Na/Ca abundance ratio only for
three objects (SDSS J095645.14+591240.6, SDSS J164939.23+223807.2 and SDSS J212312.20+001653.5).
Another potentially sodium-rich white dwarf, G77$-$50, was
analyzed by \cite{farihi2011magnetic}. They found a $\log {\rm Na/Ca}=0.7$ abundance
ratio, but this result should also be taken with a grain of salt as the magnetism of this
object complicates its analysis and the authors
explicitly noted that their sodium abundance measurement is uncertain.

\begin{figure}
    \includegraphics[width=\columnwidth]{f6.pdf}
    \caption{Elemental abundances for CI chondrites
      \citep[][filled orange circle]{lodders2003solar}, WD~J2356$-$209 (red star)
      and the DZ stars analyzed by \citet[filled black circles]{hollands2017cool}.
      The three encircled objects are those for which we found compelling evidence
      of a Na/Ca abundance ratio greater than 1.
      Note that magnetic objects in the \cite{hollands2017cool} sample
      are not shown in this figure.
      The gray line indicates how the metal abundances in WD~J2356$-$209
      would have evolved, assuming the diffusion timescales mentioned in the text.
      The distance between two gray circles on the chemical evolution track corresponds
      to 1~Myr.}
  \label{fig:diffusion_evolution}
\end{figure}

Furthermore, \cite{harris2003initial} identified a faint ($g=21.4$) DZ star in the
Sloan Digital Sky Survey (SDSS) that has a spectrum that also appears to show a broad Na line.
As WD~J2356$-$209, the visible spectrum of SDSS J133001.13+643523.7 (J1330+6435) is
dominated by a strong and broad \ion{Na}{1} D doublet. Figure \ref{fig:J1330fit} shows our best solution
for this star and Table \ref{tab:1330} lists its derived atmospheric parameters.
Note that a hydrogen-free atmosphere was assumed, since we do not have any infrared photometry to
fit the H/He ratio to an eventual infrared flux depletion.\footnote{In any case, the addition of a moderate
  amount of hydrogen (up to $\log\,{\rm H/He}=-1.5$) does not change our conclusions on the
  Na/Ca abundance ratio of this object.}
The SDSS spectrum being noisy, the Ca/He and Na/He abundance ratios are subject
to considerable uncertainties. Nonetheless, it is clear that the Na/Ca ratio of J1330+6435 is higher
than average, but well below the extreme ratio found for WD~J2356$-$209.
While there are some objects with a Na/Ca abundance ratio above the chondritic value,
WD~J2356$-$209 is the most extreme case ever encountered.

\begin{figure}
    \includegraphics[width=\columnwidth]{f7.pdf}
    \caption{Our best solution for J1330+6435. The top panel shows our fit to the visible spectrum
      and the bottom panel displays our photometric fit to the SDSS $u$ band and Pan-STARRS $grizy$ bands.
      Note that the SDSS spectrum was smoothed for clarity.}
  \label{fig:J1330fit}
\end{figure}

\begin{deluxetable}{cc}
  \tablecaption{J1330+6435 atmospheric parameters \label{tab:1330}}
  \tablehead{\colhead{\hspace{0.7cm}Parameter}\hspace{0.7cm} &
    \colhead{\hspace{0.7cm}Value}\hspace{0.7cm}}
  \startdata
  $T_{\rm eff}$       & $\phd \phn \phn 4310 \pm 190\,{\rm K}$\\
  $\log g$            & $\phn \phd 8.26 \pm 0.15$\\
  ${\rm H/He}$        & $\phn \phd 0$\\
  $\log\,{\rm Na/He}$ & $-8.5 \pm 0.3$\\
  $\log\,{\rm Ca/He}$ & $-8.8 \pm 0.3$
  \enddata
\end{deluxetable}

\subsection{Constraints on the accreted planetesimal}

The abundances of heavy elements in a DZ star are indicative of the nature of the
accreted parent body and can be used to infer its composition
\citep{zuckerman2007chemical,koester2011cool,dufour2012detailed,hollands2018cool,harrison2018polluted}.
Such studies have highlighted the existence of a great diversity of accreted bodies,
ranging from Kuiper-Belt-Object analogs \citep{xu2017chemical} to
differentiated rocky bodies \citep{zuckerman2011aluminium,melis2017differentiated}
and water-bearing planetesimals \citep{farihi2013evidence,raddi2015likely}.
Can we relate the high Na/Ca ratio of WD~J2356$-$209 to any solar system counterpart?

Table \ref{tab:naca} lists the Na/Ca ratio of a few solar system objects. The only
measurements compatible with the composition of WD~J2356$-$209 are those obtained for the
dust of the comet 67P/Churyumov-Gerasimenko (67P). Those measurements were obtained
by the COmetary Secondary Ion Mass Analyzer (COSIMA, \citealt{kissel2007cosima})
onboard the \textit{Rosetta} spacecraft while it followed comet 67P at close distances
for two years. Additionally, with the exception of Mn and Fe, the abundances of the other
heavy elements in WD~J2356$-$209
are compatible with those measured in the dust of comet 67P (Figure \ref{fig:composition}).

\begin{deluxetable}{ccc}
  \tablecaption{Sodium abundances \label{tab:naca}}
  \tablehead{\colhead{Object} & \colhead{$\log\,{\rm Na/Ca}$\tablenotemark{a}} & \colhead{Reference}}
  \startdata
  WD~J2356$-$209 & $\phn \phd 1.0 \pm 0.2$ & This paper\\
  CI chondrites & $-0.017 \pm 0.002$ & \cite{lodders2003solar} \\
  Bulk Earth & $-0.64 \pm 0.04$ & \cite{wang2018elemental} \\
  Earth's mantle & $-0.74 \pm 0.04$ & \cite{wang2018elemental}\\
  Earth's crust & \phn 0.00 & \cite{crc99}\\
  Halley & $\phn \phd 0.2 \pm 0.3$ & \cite{jessberger1988aspects}\\
  67P & $\phn \phd 1.2 \pm 0.6$ & \cite{bardyn2017carbon}
  \enddata
  \tablenotetext{a}{Ratio of number densities}
\end{deluxetable}

\begin{figure}
    \includegraphics[width=\columnwidth]{f8.pdf}
    \caption{Elemental abundances by number relative to Ca. The data for WD~J2356$-$209 is
      from Table \ref{tab:2356}, chondritic abundances are taken from
      \cite{lodders2003solar} and the data for comets Halley and 67P are from
      \cite{jessberger1988aspects} and \cite{bardyn2017carbon}, respectively.
      The upper limits represented by dotted arrows are those for which
      no firm constraint could be established. Note that the abundances
      for WD~J2356$-$209 correspond to the abundance ratios of the accreted planetesimal
      only if accretion is in its early phase (i.e., the effects of relative diffusion are
      not included in this figure).
    }
  \label{fig:composition}
\end{figure}

That being said, the total mass accreted by WD J2356$-$209 is incompatible with the mass
of a comet. By estimating the mass of metals currently in the convection zone, we can
obtain a lower limit on the total accreted mass (it is a lower limit since diffusion
might already have evacuated heavy elements from the convection zone).
Using the envelope model code of \cite{rolland2018spectral}, we find that the fractional
mass of the convection zone is $\log q=-5.49$ for a $T_{\rm eff}=4000\,{\rm K}$ white dwarf with
$\log g=8$ and $\log\,{\rm H/He}=-1.5$.
With this value, we find that the total mass in the convection zone
of the four heavy elements clearly detected in WD~J2356$-$209
(Ca, Mg, Na and Fe) is $5 \times 10^{20}\,{\rm g}$. This value could significantly
underestimate the total mass of metals currently in the convection zone,
since it does not include C, O and Si,
three elements that are expected to be particularly abundant
(Figure \ref{fig:composition}). A higher estimate can be obtained by assuming
that the accreted planetesimal had a chondritic composition relative to Ca and computing its total
mass from the abundance of Ca detected in WD~J2356$-$209. Using the
values published in \cite{lodders2003solar}, this yields a mass of $\sim 10^{21}\,{\rm g}$.
This mass is significantly higher than the mass of comet 67P
\citep[$10^{16}\,{\rm g}$,][]{patzold2016homogeneous} and that of the most massive comets
of the solar system
\citep[Hale-Bopp has a mass of $\sim 10^{19}\,{\rm g}$,][]{weissman2007cometary}, suggesting
that a single comet cannot be the cause of the pollution of the atmosphere of WD~J2356$-$209.
As the lower limit on the accreted mass is $\sim 10^2$ times higher than the mass of the
largest comets, any scenario in which several comets were accreted can safely be rejected.

\subsection{Relative diffusion}

Alternatively, it is possible that the accreted planetesimal did not have an
unusual composition and the extreme Na/Ca abundance
ratio could simply be due to the different
diffusion timescales of Na and Ca.
In fact, for a cool helium-rich white dwarf like WD~J2356$-$209, diffusion-accretion equilibrium
cannot be assumed \citep{koester2011cool,hollands2018cool}.
This follows from the fact that the diffusion
times are of the order of a few Myr
\citep{paquette1986diffusion,koester2009accretion,hollands2017cool}, while the typical
duration of an accretion episode is only of $10^4-10^6$ years
\citep{jura2008pollution,kilic2008near,melis2011accretion,girven2012constraints}.
It is therefore possible that WD~J2356$-$209 has stopped accreting and that the difference
between the diffusion timescales of Na and Ca has led to a composition that is not
representative of the accreted planetesimal.

Once the accretion episode has stopped, relative diffusion implies that a change
$\Delta \log\,{\rm Ca/He}$ will be accompanied by a variation
of the Na/Ca abundance ratio given by \citep[][Equation 3]{hollands2018cool},
\begin{equation}
  \frac{\Delta \log\,{\rm Na/Ca}}{\Delta \log\,{\rm Ca/He}} =
  \frac{\tau_{\rm Ca}}{\tau_{\rm Na}} -1.
  \label{eq:relative_diffusion}
\end{equation}
In WD~J2356$-$209, the diffusion timescale of Na is longer by a factor of $\approx 1.7$
than the diffusion timescale of Ca
($\log \tau_{\rm Ca} \approx 6.32$ and $\log \tau_{\rm Na} \approx 6.56$).\footnote{To estimate the diffusion timescales, we use the values given by
  \cite{hollands2017cool} for SDSS J163601.33+161907.1, as this star has similar
  atmospheric parameters to WD~J2356$-$209.}
From Equation \ref{eq:relative_diffusion}, it follows that every 1 dex decrease
in $\log\,{\rm Ca/He}$
is accompanied by a 0.4 increase in $\log\,{\rm Na/Ca}$. If we assume for a moment
that the accreted planetesimal had a chondritic composition with $\log\,{\rm Na/Ca}=0$,
it implies that the Ca abundance in the atmosphere of WD~J2356$-$209 was
$\log\,{\rm Ca/He}=-6.8$ when the accretion episode stopped, some $\approx 10\,{\rm Myr}$
ago \citep[][Equation 4]{kawka2016extreme}. This would raise our
lower limit on the total accreted mass to $\sim 10^{23}\,{\rm g}$, which corresponds
to the mass of a very large asteroid
\citep[Vesta has a mass of $2.6 \times 10^{23}\,{\rm g}$,][]{russell2012dawn}.
However, this scenario appears unlikely. Cool DZ stars are known to be much less
polluted than hotter objects
\citep{dufour2007spectral,koester2011cool,hollands2017cool}, possibly because the
largest planetesimals are gradually scattered away from the planetary system
\citep{veras2013simulations,veras2016full,hollands2018cool}.
In fact, according to the Montreal White Dwarf
Database \citep{dufour2016montreal}, no known DZ star cooler than
$T_{\rm eff}=5000\,{\rm K}$ has a calcium abundance higher than $\log\,{\rm Ca/He}=-9.3$.

More importantly, assuming that WD~J2356$-$209 accreted
a planetesimal with a chondritic composition might not be a realistic hypothesis.
Figure \ref{fig:diffusion_evolution} shows how the composition of WD~J2356$-$209 is expected
to have evolved given the diffusion timescales of \cite{hollands2017cool}. This
evolution rules out the possibility that the accreted planetesimal had a
chondrite-like composition. A more realistic
hypothesis would probably be to assume that the accreted planetesimal had a sodium abundance
ratio of $\log\,{\rm Na/Ca} \approx 0.6$, which corresponds to the region where
the chemical evolution track of WD~J2356$-$209 intersects the middle
of the distribution of objects plotted in Figure \ref{fig:diffusion_evolution}.
In that case, the Ca abundance in the atmosphere of WD~J2356$-$209 when the accretion
episode stopped
$\approx 4\,{\rm Myr}$ ago (i.e., $1.9 \tau_{\rm Ca}$ or $1.1 \tau_{\rm Na}$)
would have been a less extreme $\log\,{\rm Ca/He} \approx -8.3$ and
the lower limit on the accreted mass is decreased to $\sim 10^{22}\,{\rm g}$.
Assuming a typical asteroid density of $2\,{\rm g}\,{\rm cm}^{-3}$, the accreted
planetesimal had a radius of at least 100\,km.

\section{Conclusion}
\label{sec:conclusion}
We presented a detailed analysis of WD~J2356$-$209, a very cool DZ star whose
spectrum is dominated by a strong sodium feature. Thanks to our improved atmosphere models (Papers~I and II),
we find an excellent fit to the photometry and the visible spectrum, allowing the
first reliable atmospheric parameter determination of this object. We found that
WD~J2356$-$209 has a record sodium abundance with a number density ratio
$\log\,{\rm Na/Ca}=1.0 \pm 0.2$.

A possible explanation for this high sodium content is that WD~J2356$-$209 has accreted
a planetesimal with an abnormally high sodium abundance and a total mass
$\gtrsim 10^{21}\,{\rm g}$.
However, we were unable to identify a solar system analog to this hypothetical
planetesimal, since none of the examined candidates simultaneously matched the
constraints on the sodium abundance and the total mass.
Alternatively, the high sodium abundance in the atmosphere of WD~J2356$-$209 could
be explained by the slower diffusion of Na with respect to Ca. According
to this scenario, the accreted object would have had a less extreme composition
but a larger total mass ($\gtrsim 10^{22}\,{\rm g}$).

This paper concludes the observational validation of our improved
cool white dwarf model atmosphere code.
The excellent fit obtained for this extreme object is a clear demonstration of the
capacity of our models to properly take into account the nonideal effects that
prevail in the atmospheres of cool white dwarfs.
In the next paper of this series, we will use our improved models to analyze a large
sample of cool white dwarfs and revisit their spectral evolution.

\acknowledgments

We would like to thank Manuel Barranco for sharing with us ab initio potentials for the Ca$-$He interaction.
We are grateful to the anonymous reviewer for her or his valuable comments on our manuscript.
We also thank Siyi Xu for useful discussions regarding the composition of WD~J2356$-$209.

This work was supported in part by NSERC (Canada) and the Fund FRQNT (Qu\'ebec).
This work has made use of the Montreal White Dwarf Database \citep{dufour2016montreal}.

This work has made use of data from the European Space Agency (ESA) mission
{\it Gaia} (\url{https://www.cosmos.esa.int/gaia}), processed by the {\it Gaia}
Data Processing and Analysis Consortium (DPAC,
\url{https://www.cosmos.esa.int/web/gaia/dpac/consortium}). Funding for the DPAC
has been provided by national institutions, in particular the institutions
participating in the {\it Gaia} Multilateral Agreement.

The Pan-STARRS1 Surveys (PS1) and the PS1 public science archive have been made possible through contributions by the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, the Queen's University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under Grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation Grant No. AST-1238877, the University of Maryland, Eotvos Lorand University (ELTE), the Los Alamos National Laboratory, and the Gordon and Betty Moore Foundation.

This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration.

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redpajama_set_name: RedPajamaArXiv


Mackey Metal Roofing was established in 1999 by Dave Mackey. We provide our clients with the knowledge that comes from 13+ years of hands-on metal roofing and siding installation, materials specification and supply, and product support.
Mackey Metal Roofing (MMR) was exclusively a metal roofing contracting business working in Vermont, New York, Ontario and Quebec, and was well known for delivering complex residential projects with a lot of detail (skylights, valleys, chimneys, intersecting roof lines, multiple pitches, windows, walls and issues re snow, ice and ventilation).
In 2008 it became clear that there was a need in the market for a company that could supply both materials AND expertise to contractors and homeowners. Today, 13 years later, MMR is a supplier of metal roofing, siding, trim, accessories and industry related materials to contractors and home owners in the USA and parts of Canada. Additionally, we prepare materials lists, train contractors and homeowners, and provide technical / installation support via phone, email and video to our clients located throughout North America. We are involved from supply to construction, working closely with our suppliers to ensure that orders are accurate and delivered on time, and helping our clients find solutions to the inevitable complexities that present themselves during construction. We are proud distributors for American Building Components (established in 1908), Penn Valley Paint (makers of the Calbar line of metal roof paints since 1927), LevelRite ladder tools, Sno-Blox snow retention systems and EagleView aerial roof measuring.
With the exception of the power tools that we carry, all of the products that we sell are manufactured in the USA by American-owned companies that support their local communities by providing gainful employment, purchasing materials from local suppliers, paying municipal, state and federal taxes and playing an active role in various support organizations.
We are passionate about what we do, are viewed as true professionals in the industry and consider the opportunity to work for our customers a privilege. Metal roofing has the potential to last well into our children's lifetimes, something that we take to heart in every interaction and transaction to ensure that any and all expectations are met…and exceeded.