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User talk:Varangian

 * Name: Kristian
 * Nationality: Canada
 * Location: Reading, Berkshire, United Kingdom
 * Contributing in Wikipedia since July 20, 2003
 * Security Consultant

Byz. aristocracy
Hello Varangian! Thanks for the comments, but I am a bit puzzled by what you wrote. It is clearly mentioned in the opening paragraph where this table came from (Taktikon Uspensky, Kletorologion, etc.), and most titles are cited from Bury's excellent book, which is precisely on the Kletorologion. Anyhow, the page still requires a lot of work. I intend to divide it into periods, namely late Roman (the senatorial ranks, namely clarissimi, illustres, etc.), middle Byzantine (essentially there), Komnenian (sebastoi etc) and Palaiologan (based on pseudo-Kodinos), where the difference between title and office vanishes. I would however appreciate any input or assistance, especially on how it reads to a third-party reader, i.e. if the text is understandable and the hierarchy, evolution and interrelation of ranks is clear. Regards, Constantine  ✍  20:31, 7 May 2009 (UTC)

Bureau of Barbarians

 * Hey man. You have contributed to the article Bureau of Barbarians. Essentially, there is no factual or textual evidence AT ALL that there was ever a formalised spying bureau in Byzantium. There was a Bureau mentioned in the Notitia Dignitatum of the fifth century [see Otto Seeck, Notitia Dignitatum accedunt Notitia Urbis Constantinopolitanae Laterculi Prouinciarum (Berlin, Apud Weidmannos 1876) pp 31-33.] But no mentions in any text after this point. So, unless you can dazzle me with some evidence substantiating you calling the bureau the "world's first intelligence agency", I think you are peddling fantasy. Varangian (talk) 11:54, 11 May 2009 (UTC)

Thanks for the feedback. But you have rewritten the article to deliberately push your point of view which is inappropriate. If you felt the article as written was biased you should have balanced the bias, not replaced it with your own bias.

I provided a list of references that characterize the department in the way that I had in the article, references which you chose to remove. Granted some of these are not as authoritative as I would like but it is hard to find a lot of research on the subject (hence the reason it has remained a stub article).

I appreciate your efforts to improve the article but I think you need to be more careful in your edits. I agree, though, that the history of this department and its role is very unclear and you obviously have more of a command of the history than I do. But the point of view you are pushing, while it may be correct, is not universally held.

--Mcorazao (talk) 14:55, 12 May 2009 (UTC)

 * Okay, apologies for coming across as harsh, I shouldn't have been, and you ought to be commended for doing some reading and putting the links: this is far better than most people do. Still, your sources are not just weak but tenuous to the extreme. It is not that I am pushing a POV, but rather that I am writing to the existing evidence. One must not take things further than the evidence bears no matter how nifty an alternative might seem. All the best, Varangian (talk) 15:54, 12 May 2009 (UTC)

I appreciate your efforts at diplomacy and I recognize that your efforts are well-intentioned.

Nevertheless, my concerns still stand. We can quibble over semantics but statements such as "There is however no evidence" are Original Research unless you attribute them to an authoritative source which is reasonably representative of scholarly consensus on the subject. Otherwise it is inappropriate regardless of whether it is true. You seem to be drawing a lot of conclusions from your own interpretation of this one source.

In any event, I agree that, as written, this was not a good article and that the sources are poor. But it was only a stub. Let's just make sure we are taking steps in a positive direction as we edit.

--Mcorazao (talk) 15:26, 13 May 2009 (UTC)

 * ''Bureau of Barbarians III=

Well, one cannot prove a negative: the absence of evidence is not the evidence of absence, so you are right to say that one can not be absolute when saying the Bureau was not an espionage agency. Yet, the converse is that lack of evidence does not prove conspiracy. I think between Constantine and me we do not say defintely they were NOT, only noting that there is a lack of evidence to prove that it was, noting the weakness of the opposing argument, and suggesting the Agentes in rebus as a more likely, but still unlikely, candidate for the position. We do note the Bureau's intelligence (not espionage) function. And if you look, you'll it IS original research: we are quoting all the relevant and exisiting primary sources: Procopius, Theophanes, the Theodosian & Justinian Codes, and the main edited secondary texts by Bury, JP Migne, Khazdan, Brehier, etc. Our arguments are on firm evidenciary footings. KC Gustafson (talk) 16:05, 14 May 2009 (UTC)''

Well, we're now getting into some subtleties:
 * Disproving negatives: The point is that knowledgeable authors do characterize the Bureau as an intelligence agency. So suggesting based on your own reading of texts that it is not would be inappropriate. Suggesting that there is disagreement and that the full role of the department was unclear is, however, very appropriate.
 * Intelligence vs. espionage: I think you are trying to draw some distinctions which, most likely, the Byzantines would not have even understood. I have not seen anyone state that the Bureau was conducting major Bay-of-Pigs-type operations or anything like that if this is what you mean. But they certainly gathered intelligence by spying on foreigners within the Empire. You can argue that their "spying" was not quite the same as the modern art of espionage which is true but it is clear it was far more sophisticated than simply happening to overhear a few things. The Bureau was clearly (to varying degrees) engaged in deliberate efforts to gain intelligence from and manipulate foreign assets and dignataries for the purpose of state security. You can say that their methods were not the same as or nearly so sophisticated as modern "intelligence agencies" but there was clearly an organized effort to accomplish similar goals.

Another subtlety which I think you are implying is that the Bureau was diplomatic in nature and so it is improper to assign it an identity as an espionage organization. If that is the case then I believe you are trying to cast things in the light of how modern governments organize themselves. Modern governments normally have explicit branches separately tasked with diplomacy and intelligence gathering. Of course, even in modern governments embassies are commonly used both for diplomacy and as bases of espionage. In Byzantine times, though, these things were even more murky.

--Mcorazao (talk) 16:49, 14 May 2009 (UTC)

Patriarchs
Hello Varangian, long time no see! I hope you are well! You are quite right, the patriarch articles are horribly deficient both in quantity and in quality. I do intend to bring them up to scratch eventually, but I cannot really help, because a) I have very limited time due to RL concerns and b) I have dozens of other articles I intend to work on/am working on, and c) frankly, patriarchs and religious matters in general are not my priority or forte. As for organizing a community effort, sadly the users who work on Byzantine articles are a handful, and no one really works on such pages either. Plus, there is really no forum for making such a request. You might try recruiting some editors at the Middle Ages, Greece and Orthodoxy Wikiprojects, but I'd be surprised if more than one or two users reply. It's as usual here at WP, if you want something done, best go ahead and do it yourself. I can help occasionally and point you to some sources, if you want, but that's about it for now. Constantine  ✍  13:13, 21 January 2011 (UTC)

 * Hah, well, my contributions to most patriarch articles are slight copyedits, adding templates & categories, as I've done with most Byzantine-related articles. Nothing too demanding or time-consuming. When I say that they are not my forte, I mean it: the various religious disputes they were involved in, and which are essential in writing articles on them, bore me immensely. On your last question, the answer is "by using every free moment". Luckily I usually work on a computer, so it's easy to drop in and check WP rather often (as well as to have some handy sources ready in a flash drive) ;). Cheers, Constantine  ✍  08:27, 24 January 2011 (UTC)

 * You are most certainly correct in what you say, and I agree 100% with you. The difference is, I had Orthodox religion classes at school, and had to learn tons of useless stuff of this nature, even during Byzantine history classes, which almost ruined the Byzantine period for ever for me. Don't get me wrong, all religions fascinate me, but in this case the dislike is practically visceral ;). Cheers, Constantine  ✍  20:55, 27 January 2011 (UTC)

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title: User talk:Varangian


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Little egret

The little egret (Egretta garzetta) is a species of small heron in the family Ardeidae. It is a white bird with a slender black beak, long black legs and, in the western race, yellow feet. As an aquatic bird, it feeds in shallow water and on land, consuming a variety of small creatures. It breeds colonially, often with other species of water birds, making a platform nest of sticks in a tree, bush or reed bed. A clutch of three to five bluish-green eggs is laid and incubated by both parents for about three weeks. The young fledge at about six weeks of age.

Its breeding distribution is in wetlands in warm temperate to tropical parts of Asia, Africa, Australia, and Europe. A successful colonist, its range has gradually expanded north, with stable and self-sustaining populations now present in the United Kingdom.

In warmer locations, most birds are permanent residents; northern populations, including many European birds, migrate to Africa and southern Asia to over-winter there. The birds may also wander north in late summer after the breeding season, and their tendency to disperse may have assisted in the recent expansion of the bird's range. At one time common in Western Europe, it was hunted extensively in the 19th century to provide plumes for the decoration of hats and became locally extinct in northwestern Europe and scarce in the south. Around 1950, conservation laws were introduced in southern Europe to protect the species and their numbers began to increase. By the beginning of the 21st century the bird was breeding again in France, the Netherlands, Ireland and Britain. Its range is continuing to expand westward, and the species has begun to colonise the New World; it was first seen in Barbados in 1954 and first bred there in 1994. The International Union for Conservation of Nature has assessed the bird's global conservation status as being of "least concern".

Taxonomy
The little egret was formally described by the Swedish naturalist Carl Linnaeus in 1766 in the twelfth edition of his Systema Naturae under the binomial name Ardea garzetta. It is now placed with 12 other species in the genus Egretta that was introduced in 1817 by the German naturalist Johann Reinhold Forster with the little egret as the type species. The genus name comes from the Provençal French Aigrette, "egret", a diminutive of Aigron, "heron". The species epithet garzetta is from the Italian name for this bird, garzetta or sgarzetta.

Two subspecies are recognised:
 * E. g. garzetta (Linnaeus, 1766) – nominate, found in Europe, Africa, and most of Asia except the south-east
 * E. g. nigripes (Temminck, 1840) – found in the Sunda Islands, Australia and New Zealand

Three other egret taxa have at times been classified as subspecies of the little egret in the past but are now regarded as two separate species. These are the western reef heron Egretta gularis which occurs on the coastline of West Africa (Egretta gularis gularis) and from the Red Sea to India (Egretta gularis schistacea), and the dimorphic egret (Egretta dimorpha), found in East Africa, Madagascar, the Comoros and the Aldabra Islands.

Description
The adult little egret is 55 – long with an 88 – wingspan, and weighs 350 –. Its plumage is normally entirely white, although there are dark forms with largely bluish-grey plumage. In the breeding season, the adult has two long plumes on the nape that form a crest. These plumes are about 150 mm and are pointed and very narrow. There are similar feathers on the breast, but the barbs are more widely spread. There are also several elongated scapular feathers that have long loose barbs and may be 200 mm long. During the winter the plumage is similar but the scapulars are shorter and more normal in appearance. The bill is long and slender and it and the lores are black. There is an area of greenish-grey bare skin at the base of the lower mandible and around the eye which has a yellow iris. The legs are black and the feet yellow. Juveniles are similar to non-breeding adults but have greenish-black legs and duller yellow feet, and may have a certain proportion of greyish or brownish feathers. The subspecies nigripes differs in having yellow skin between the bill and eye, and blackish feet. During the height of courtship, the lores turn red and the feet of the yellow-footed races turn red.

Little egrets are mostly silent but make various croaking and bubbling calls at their breeding colonies and produce a harsh alarm call when disturbed. To the human ear, the sounds are indistinguishable from the black-crowned night heron (Nycticorax nycticorax) and the cattle egret (Bubulcus ibis) with which it sometimes associates.

Distribution and habitat
The breeding range of the western race (E. g. garzetta) includes southern Europe, the Middle East, much of Africa and southern Asia. Northern European populations are migratory, mostly travelling to Africa although some remain in southern Europe, while some Asian populations migrate to the Philippines. The eastern race, (E. g. nigripes), is resident in Indonesia and New Guinea, while E. g. immaculata inhabits Australia and New Zealand, but does not breed in the latter. During the late twentieth century, the range of the little egret expanded northwards in Europe and into the New World, where a breeding population was established on Barbados in 1994. The birds have since spread elsewhere in the Caribbean region and on the Atlantic coast of the United States.

The little egret's habitat varies widely, and includes the shores of lakes, rivers, canals, ponds, lagoons, marshes and flooded land, the bird preferring open locations to dense cover. On the coast it inhabits mangrove areas, swamps, mudflats, sandy beaches and reefs. Rice fields are an important habitat in Italy, and coastal and mangrove areas are important in Africa. The bird often moves about among cattle or other hoofed mammals.

Behaviour
Little egrets are sociable birds and are often seen in small flocks. Nevertheless, individual birds do not tolerate others coming too close to their chosen feeding site, though this depends on the abundance of prey.

Food and feeding
They use a variety of methods to procure their food; they stalk their prey in shallow water, often running with raised wings or shuffling their feet to disturb small fish, or may stand still and wait to ambush prey. They make use of opportunities provided by cormorants disturbing fish or humans attracting fish by throwing bread into water. On land they walk or run while chasing their prey, feed on creatures disturbed by grazing livestock and ticks on the livestock, and even scavenge. Their diet is mainly fish, but amphibians, small reptiles, mammals and birds are also eaten, as well as crustaceans, molluscs, insects, spiders and worms.

Breeding
Little egrets nest in colonies, often with other wading birds. On the coasts of western India these colonies may be in urban areas, and associated birds include cattle egrets (Bubulcus ibis), black-crowned night herons (Nycticorax nycticorax) and black-headed ibises (Threskiornis melanocephalus). In Europe, associated species may be squacco herons (Ardeola ralloides), cattle egrets, black-crowned night herons and glossy ibises (Plegadis falcinellus). The nests are usually platforms of sticks built in trees or shrubs, or in reed beds or bamboo groves. In some locations such as the Cape Verde Islands, the birds nest on cliffs. Pairs defend a small breeding territory, usually extending around 3 to 4 m from the nest. The three to five eggs are incubated by both adults for 21 to 25 days before hatching. They are oval in shape and have a pale, non-glossy, blue-green shell colour. The young birds are covered in white down feathers, are cared for by both parents and fledge after 40 to 45 days.

Conservation
Globally, the little egret is not listed as a threatened species and has in fact expanded its range over the last few decades. The International Union for Conservation of Nature states that their wide distribution and large total population means that they are a species that cause them "least concern".

Status in northwestern Europe
Historical research has shown that the little egret was once present, and probably common, in Ireland and Great Britain, but became extinct there through a combination of over-hunting in the late medieval period and climate change at the start of the Little Ice Age. The inclusion of 1,000 egrets (among numerous other birds) in the banquet to celebrate the enthronement of George Neville as Archbishop of York at Cawood Castle in 1465 indicates the presence of a sizable population in northern England at the time, and they are also listed in the coronation feast of King Henry VI in 1429. They had become scarce by the mid-16th century, when William Gowreley, "yeoman purveyor to the Kinges mowthe", "had to send further south" for egrets. In 1804 Thomas Bewick commented that if it were the same bird as listed in Neville's bill of fare "No wonder this species has become nearly extinct in this country!"

Further declines occurred throughout Europe as the plumes of the little egret and other egrets were in demand for decorating hats. They had been used in the plume trade since at least the 17th century but in the 19th century it became a major craze and the number of egret skins passing through dealers reached into the millions. Complete statistics do not exist, but in the first three months of 1885, 750,000 egret skins were sold in London, while in 1887 one London dealer sold 2 million egret skins. Egret farms were set up where the birds could be plucked without being killed but most of the supply of so-called "Osprey plumes" was obtained by hunting, which reduced the population of the species to dangerously low levels and stimulated the establishment of Britain's Royal Society for the Protection of Birds in 1889.

By the 1950s, the little egret had become restricted to southern Europe, and conservation laws protecting the species were introduced. This allowed the population to rebound strongly; over the next few decades it became increasingly common in western France and later on the north coast. It bred in the Netherlands in 1979 with further breeding from the 1990s onward. About 22,700 pairs are thought to breed in Europe, with populations stable or increasing in Spain, France and Italy but decreasing in Greece.

In Britain it was a rare vagrant from its 16th-century disappearance until the late 20th century, and did not breed. It has however recently become a regular breeding species and is commonly present, often in large numbers, at favoured coastal sites. The first recent breeding record in England was on Brownsea Island in Dorset in 1996, and the species bred in Wales for the first time in 2002. The population increase has been rapid subsequently, with over 750 pairs breeding in nearly 70 colonies in 2008, and a post-breeding total of 4,540 birds in September 2008. The first record of breeding in Scotland happened in 2020 in Dumfries & Galloway. In Ireland, the species bred for the first time in 1997 at a site in County Cork and the population has also expanded rapidly since, breeding in most Irish counties by 2010. Severe winter weather in 2010–2012 proved to be only a temporary setback, and the species continues to spread.

Status in Australia
In Australia, its status varies from state to state. It is listed as "Threatened" on the Victorian Flora and Fauna Guarantee Act 1988. Under this act, an Action Statement for the recovery and future management of this species has been prepared. On the 2007 advisory list of threatened vertebrate fauna in Victoria, the little egret is listed as endangered.

Colonisation of the New World
With its range continuing to expand, the little egret has now started to colonise the New World. The first record there was on Barbados in April 1954. The bird began breeding on the island in 1994 and now also breeds in the Bahamas. They may have made the crossing from Western Africa. Ringed birds from Spain provide a clue to the birds' origin. The birds are very similar in appearance to the snowy egret and share colonial nesting sites with these birds in Barbados, where they are both recent arrivals. The little egrets are larger, have more varied foraging strategies and exert dominance over feeding sites.

Little egrets are seen with increasing regularity over a wider area and have been observed from Suriname and Brazil in the south to Newfoundland, Quebec and Ontario in the north. Birds on the east coast of North America are thought to have moved north with snowy egrets from the Caribbean. In June 2011, a little egret was spotted in Maine, in the Scarborough Marsh, near the Audubon Center.

license: Creative Commons - Attribution Share-Alike - https://creativecommons.org/licenses/by-sa/4.0/

title: Little egret


text:
User talk:Lee Cremeans

Quantum Page
Hi Lee. My name is Bob Wientzen and manage PR at Quantum. Quantum has evolved greatly since the creation of our Wikipedia entry and I’m hoping to work with the Wikipedia community to update the content so that it’s reflective of the company’s current state and offerings.

I understand the importance of keeping this page factual and up-to-date for readers, thus I am happy to receive any feedback you have to ensure that this entry is current. To begin with, I would like to know your thoughts on revising the format of the entry to include the sections outlined below. Please let me know if this is an agreeable starting point for updating this entry – you can contact me directly at bob.wientzen@quantum.com.

I. Company History

II. Products/Services a. Disk-based systems/devices b. Data management software c. Tape systems, drives and media

III. Partners

IV. Company Milestones/Acquisitions (to include the acquisitions listed in the “Transformation” section) Bob Wientzen (talk) 22:19, 25 November 2009 (UTC) 146.174.255.100 (talk) 17:28, 16 December 2009 (UTC)

Hello Lee, welcome to Wikipedia. I realise you've been here for a few months as a non-logged on user, but welcome anyway! I hope you continue to enjoy editing here and being a Wikipedian.

Here are some useful links if you haven't already found them
 * How to edit a page
 * Naming conventions
 * Manual of Style
 * Help
 * Village pump

Angela 16:08 20 Jul 2003 (UTC)

---

testing my signature

-lee 03:57 27 Jul 2003 (UTC)

Hello Lee, welcome to Wikipedia. I realise you've been here for a few months as a non-logged on user, but welcome anyway! I hope you continue to enjoy editing here and being a Wikipedian.

Here are some useful links if you haven't already found them
 * How to edit a page
 * Naming conventions
 * Manual of Style
 * Help
 * Village pump

Angela 16:08 20 Jul 2003 (UTC)

---

testing my signature

-lee 03:57 27 Jul 2003 (UTC)

Old World ROM
Wow, nice rewrite there, lots of details I didn't know! --tooki 02:00, 17 Aug 2004 (UTC)
 * Thanks! I'm also going to work on some of the Mac-specific stuff that's linked from there; one of those pages (User:Lee Cremeans/Parameter RAM) is almost ready, and I plan to write something for Chimes of Death as well. -lee 22:22, 26 Aug 2004 (UTC)

ABC edit
Lee, your edit on the page looks great. I didn't even know where to start; thanks for making a big, difficult project so much easier. Keep up the contribs! :)--Firsfron 03:35, 19 Jan 2005 (UTC)
 * Thanks! -lee 20:37, 19 Jan 2005 (UTC)

Wavetable synthesis
hi lee,

i just wanted to say that i am one contributor to the Wavetable synthesis article as well as the Additive synthesis article. i was not the one to put the reference to my Wavetable Synthesis 101 paper, but when i discovered it (from a Google search), i did tweak the pages to make them more accurate.

we can revert the Wavetable synth article back to saying it is simply PCM sample playback (what the soundcards do), but if that's done i would really like any reference to my article taken out. even keeping it as it is, we could make the reference to my paper a simple "External Link" reference.

just FYI. r b-j 05:26, 31 August 2005 (UTC)
 * Looking over the artcile again, it looks like the article is fine as-is; I'll go ahead and remove the cleanup tag, and move the link as you suggested. -lee 02:09, 1 September 2005 (UTC)

 * Lee, i just noticed that the definition of Wavetable synthesis got essentially reverted back to mean "PCM sample playback". We need to figure out a way to include both definitions and their context and to make sure we differentiate them for the reader because they are not the same.  Are you willing to work with me on that?  Please take a look at Talk:Wavetable synthesis and get back to me there, okay? r b-j 01:44, 3 February 2006 (UTC)

Fairfax County Water Authority
It looks like a pretty good article about a notable company. However, it seems to be missing some sources. Could you note where you got all the information in the article? The official web site doesn't seem to have all of it. Thanks. Superm401 | Talk 23:08, 4 December 2005 (UTC)
 * Most of what I know about them came from a history page they had posted on an old version of their web site. Since most of it is from memory (and the page in question is long gone), I decided a couple of weeks ago to go back into the Washington Post archives and do some research; it turns out most of what I remember is inaccurate and/or incomplete, so I'll be rewriting it and adding references soon. -lee 18:43, 5 December 2005 (UTC)

How are the re-writes coming? I'm working in a similar category (NoVa sewage treatment to discuss the reasoanbly unique role of the UOSA in providing recycled sewage as drinking wateR) and would like to add some cross-references. Thanks! Slapshot24 20:55, 2 January 2006 (UTC)
 * It's admittedly been kind of slow, what with the holidays (and me just being lazy ;_;), but I should be able to finish it soon. The cross-references should be fine. -lee 14:24, 3 January 2006 (UTC)

Quantum Corporation

 * I saw your notes and additions on the Quantum article, but I also had a few questions (which I left on the talk page), and I also notice someone from a Maxtor Shrewsbury IP has shown up and made some rather NPOV edits. Are there any public sources for any of this? -lee 23:50, 12 May 2006 (UTC)

 * There are probably no public sources for this information. I worked in engineering at Quantum Corporation during the late 1990s to early 2000s and had an insider's view of company politics, as well as proprietary information about design details and documentation.  The NPOV comments that were added by anonymous user 134.6.234.211 after I posted my series of notes are pure spin and wishful thinking.  —QuicksilverT @ 20:34, 1 June 2006 (UTC)
 * Ah, I figured as much. Thanks... -lee 01:33, 2 June 2006 (UTC)

Now that it's a good article...
...I'm giving you huggable, very special, overdue thanks from me and the Care Bear Family for starting the page on The Care Bears Movie way back in July 2004. Plus, $25 worth of Wikicash to spend wisely when you return to this wiki.

I wish you a happy summer...and happy editing! --Slgrandson 02:42, 13 June 2006 (UTC)

DC Meetup notice
Greetings. There is going to be a Washington DC Wikipedia meetup on next Saturday, July 21st at 5pm in DC. Since you are listed in Category:Wikipedians_in_Virginia, I thought I'd invite you to come. I'm sorry about the short notice for the meeting. Hopefully we'll do somewhat better in that regard next time. If you can't come but want to make sure that you are informed of future meetings be sure to list yourself under "but let me know about future events", and if you don't want to get any future direct notices \(like this one\), you can list yourself under "I'm not interested in attending any others either" on the DC meetup page.--Gmaxwell 22:08, 14 July 2007 (UTC)

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DC Meetup on May 17th
Your help is needed in planning Meetup/DC 4! Any comments or suggestions you have are greatly appreciated. The Placebo Effect (talk) 19:49, 8 March 2008 (UTC)

New World ROM
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You're invited...
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DC Meetup Events: You're invited!
This has been an automated because you your name was on the invite list. BrownBot (talk) 16:34, 21 February 2009 (UTC)

Recent edits to the Conner Page
Hi Lee: Since u and I have worked together on the Conner page, I would appreciate your review of the recent edits I made to the page. Tom94022 (talk) 19:25, 22 April 2009 (UTC)
 * Looks good; I read that article too, and enjoyed it thoroughly. :) -lee (talk) 16:24, 6 November 2009 (UTC)

Planning Discussions Now Finished Regarding DC Meetup #9
--NBahn (talk) 02:40, 10 December 2009 (UTC)
 * You are receiving this message either because you received a similar one before and didn't object, or you requested to receive a similar one in the future. If you don't wish to receive this message again, then please let me know either on my talk page or here.
 * Planning — for the most part, anyway — is now finished (see here) for DC Meetup #9.

Planning Discussions Now Underway Regarding DC Meetup #10

 * You are receiving this message either because you received a similar one before and didn't object, or you requested to receive a similar one in the future. If you don't wish to receive this message again, then please let me know either on my talk page or here.
 * Please be advised that planning is now underway (see here) for DC Meetup #10. --NBahn (talk) 15:21, 7 May 2010 (UTC)

Meetup/DC 11
Hey, just in case you missed it, there is an oppurtunity to get a free dinner this Tuesday August 11 and a chance to meet and hang out talk about WikiProject United States Public Policy and WP:GLAM/SI. Sorry that this is so late in the game, I was hoping the e-mail would be a better form of contact for active members (if you want to get on the e-mail list send me an User e-mail ). Hope that you can attend, User:Sadads (talk)12:10, 9 August 2010 (UTC)

DC Meetup #12
An off-wiki discussion is taking place concerning DC Meetup #12. Watch this page for announcements.

—NBahn (talk) 04:35, 9 September 2010 (UTC)

P.S. You are receiving this message either because you received a similar one before and didn't object, or you requested to receive a similar one in the future. If you don't wish to receive this message again, then please let me know either on my talk page or here.

S-LCD edit
Just letting you know that removing the forum-y bits from S-LCD is allowed. The revert as vandalism appeared to be in error. Thanks for helping try to clean up this page! – GorillaWarfare (talk) 22:03, 30 March 2012 (UTC)
 * Thanks for the clarification. It's been a while since I've done a lot of editing here, so I'm still getting re-acquainted. -lee (talk) 21:25, 12 June 2012 (UTC)

You are invited to the "All Things GW" editathon on Saturday, April 20
The "All Things GW" editathon on Saturday, April 20, 2013 from 12:30 p.m. to 4:00 p.m. is a rare chance to go behind the scenes in the University Archives of the GW Libraries and use their unique resources to research and update Wikipedia pages related to The George Washington University and the Foggy Bottom neighborhood. Did you miss our last D.C. history editathon? This is your is your chance to come edit with wiki-friends using different great collection! The event includes a behind-the-scenes tour of the University Archives and a show-and-tell of some of its most interesting treasures, snacks, and the editathon.

Participation is limited to 30 volunteers, so RSVP today! Dominic·t 07:22, 15 April 2013 (UTC)

Webinar / edit-a-thon at the National Library of Medicine (NLM)
Join us at the NLM next week, either in person or online, to learn about NLM resources, hear some great speakers, and do some editing!

On Tuesday, 28 May there will be a community Wikipedia meeting at the United States National Library of Medicine in Bethesda, Maryland - with a second on Thursday, 30 May for those who can't make it on Tuesday. You can participate either in-person, or via an online webinar. If you attend in person, USB sticks (but not external drives) are ok to use.

Please go to the event page to get more information, including a detailed program schedule.

If you are interested in participating, please register by sending an email to pmhmeet@gmail.com. Please indicate if you are coming in person or if you will be joining us via the webinar. After registering, you will receive additional information about how to get to our campus (if coming in-person) and details about how to join the webinar. Klortho (talk) 05:48, 25 May 2013 (UTC)

Have time on Saturday?
I'm sorry for the last-minute notice, but on Saturday, June 8, from 3 to 6 PM, Wikimedia DC and the Cato Institute are hosting a Legislative Data Meetup. We will discuss the work done so far by WikiProject U.S. Federal Government Legislative Data to put data from Congress onto Wikipedia, as well as what more needs to be done. If you have ideas you'd like to contribute, or if you're just curious and feel like meeting up with other Wikipedians, you are welcome to come! Be sure to RSVP here if you're interested.

I hope to see you there!

(You can unsubscribe from future notifications for D.C.-area events by removing your name from this list.)

Harej (talk) 04:15, 6 June 2013 (UTC)

DC meetup & dinner on Saturday, June 15!
Please join Wikimedia DC for a social meetup and dinner at Vapiano (near Farragut North/Farragut West) on Saturday, June 15 at 5:30 PM. All Wikipedia/Wikimedia and free knowledge/culture enthusiasts, regardless of editing experience, are welcome to attend! All ages welcome!

For more information and to sign up, please see the meetup page. Hope to see you there! Kirill [talk] 19:45, 10 June 2013 (UTC)

Join us this Sunday for the Great American Wiknic!
Boilerplate message generously borrowed from Wikimedia NYC. To unsubscribe from future DC area event notifications, remove your name from this list.

Harej (talk) 15:39, 19 June 2013 (UTC)

DC meetup & dinner on Saturday, July 13!
Please join Wikimedia DC for a social meetup and dinner at Vapiano (near Farragut North/Farragut West) on Saturday, July 13 at 6:00 PM. All Wikipedia/Wikimedia and free knowledge/culture enthusiasts, regardless of editing experience, are welcome to attend! All ages welcome!

For more information and to sign up, please see the meetup page. Hope to see you there! Kirill [talk] 00:19, 6 July 2013 (UTC)

DC meetup & dinner on Saturday, August 24!
Please join Wikimedia DC for a social meetup and dinner at Vapiano (near Farragut North/Farragut West) on Saturday, August 24 at 6:00 PM. All Wikipedia/Wikimedia and free knowledge/culture enthusiasts, regardless of editing experience, are welcome to attend! All ages welcome!

For more information and to sign up, please see the meetup page. Hope to see you there! Kirill [talk] 04:00, 8 August 2013 (UTC)

Are you free on Wednesday? Join us at the Wikimedia DC WikiSalon!
Wikimedia DC invites you to join us for our next DC WikiSalon, which will be held on the evening of Wednesday, August 24 at our K Street office.

The WikiSalon an informal gathering of Wikimedia enthusiasts, who come together to discuss the Wikimedia projects and collaboratively edit. There's no set agenda, and guests are welcome to recommend articles for the group to edit or edit on their own. Light refreshments will be provided.

We look forward to seeing you there! Kirill [talk] 11:35, 19 August 2013 (UTC)

Meet up with local Wikipedians on September 14!
Are you free on Saturday, September 14? If so, please join Wikimedia DC and local Wikipedians for a social meetup and dinner at Vapiano (near Farragut North/Farragut West) at 6:00 PM. All Wikipedia/Wikimedia and free knowledge/culture enthusiasts, regardless of editing experience, are welcome to attend! All ages are welcome!

For more information and to sign up, please visit the meetup page. Hope to see you there! Kirill [talk] 18:52, 25 August 2013 (UTC)

Are you free next Thursday? Join us at the Wikimedia DC WikiSalon!
Wikimedia DC invites you to join us for our next WikiSalon, which will be held from 7 to 9 PM on Thursday, September 5 at our K Street office.

The WikiSalon is an informal gathering of Wikimedia enthusiasts, who come together to discuss the Wikimedia projects and collaboratively edit. There's no set agenda, and guests are welcome to recommend articles for the group to edit or edit on their own. Light refreshments will be provided.

We look forward to seeing you there! Kirill [talk] 14:51, 28 August 2013 (UTC)

Are you free next Thursday? Join us at the Wikimedia DC WikiSalon!
Wikimedia DC invites you to join us for our next WikiSalon, which will be held from 7 to 9 PM on Thursday, September 26 at our K Street office.

The WikiSalon is an informal gathering of Wikimedia enthusiasts, who come together to discuss the Wikimedia projects and collaboratively edit. There's no set agenda, and guests are welcome to recommend articles for the group to edit or edit on their own. Light refreshments will be provided.

We look forward to seeing you there! Kirill [talk] 05:47, 17 September 2013 (UTC)

Are you free on Sunday? Join us for a special Wikimedia DC WikiSalon!
Wikimedia DC invites you to join us for a special WikiSalon at the Martin Luther King, Jr. Memorial Library's Digital Commons Center. We will gather at 3 PM on Sunday, October 13, 2013 to discuss an important topic: what can Wikipedia and the DC area do to help each other? We hope to hear your thoughts and suggestions; if you have an idea you would like to pursue, please let us know and we will help!

Following the WikiSalon, we will be having dinner at a nearby restaurant, Ella's Wood Fired Pizza.

If you're interested in attending, please sign up at the event page. We look forward to seeing you there! Kirill [talk] 02:06, 8 October 2013 (UTC)

Meetups coming up in DC!
Hey!

You are invited to two upcoming events in DC:

 * Meetup at Capitol City Brewery on Saturday, January 25 at 6 PM. Please join us for dinner, drinks, socializing, and discussing Wikimedia DC activities and events. All are welcome! RSVP on the linked page or through Meetup.
 * Art and Feminism Edit-a-Thon on Saturday, February 1 from Noon – 5 PM. Join us as we improve articles on notable women in history! All are welcome, regardless of age or level of editing experience. RSVP on the linked page or through Meetup.

I hope to see you there!

(Note: If you do not wish to receive talk page messages for DC meetups, you are welcome to remove your username from this page.)

Harej (talk) 00:07, 16 January 2014 (UTC)

Coming up in February!
Hello there!

Our February WikiSalon is coming up on Sunday, February 23. Join us at our gathering of Wikipedia enthusiasts at the Kogod Courtyard of the National Portrait Gallery with an optional dinner after. As usual, all are welcome. Care to join us?

Also, if you are available, there is an American Art Edit-a-thon being held at the Smithsonian American Art Museum with Professor Andrew Lih's COMM-535 class at American University on Tuesday, February 11 from 2 to 5 PM. Please RSVP on the linked page if you are interested.

If you have any ideas or preferences for meetups, please let us know at Wikipedia talk:Meetup/DC.

Thank you, and hope to see you at our upcoming events! Harej (talk) 18:41, 4 February 2014 (UTC)

DC Meetups in March
 Happy March!

Though we have a massive snowstorm coming up, spring is just around the corner! Personally, I am looking forward to warmer weather.

Wikimedia DC is looking forward to a spring full of cool and exciting activities. In March, we have coming up:

 * Evening WikiSalon on Wednesday, March 12 from 7 PM – 9 PM. Meet up with Wikipedians for coffee at the Cove co-working space in Dupont Circle! If you cannot make it in the evening, join us at our...
 * March Meetup on Sunday, March 23 from 3 PM – 6 PM. Our monthly weekend meetup, same place as last month. Meet really cool and interesting people!
 * Women in the Arts 2014 meetup and edit-a-thon on Sunday, March 30 from 10 AM – 5 PM. Our second annual Women in the Arts edit-a-thon, held at the National Museum of Women in the Arts. Free lunch will be served!

We hope to see you at our upcoming events! If you have any questions, feel free to ask on my talk page.

— Harej (talk) 05:11, 3 March 2014 (UTC)

An exciting month of wiki events!
 Hello there,

I am pleased to say that April will be a very exciting month for Wikipedia in Washington, DC. We have a lot of different events coming up, so you will have a lot to choose from.

First, a reminder that our second annual Women in the Arts Edit-a-Thon will take place on Sunday, March 30 at the National Museum of Women in the Arts.

Coming up in April, we have our first-ever Open Government WikiHack with the Sunlight Foundation on April 5–6! We are working together to use open government data to improve the Wikimedia projects, and we would love your help. All are welcome, regardless of coding or editing experience. We will also be having a happy hour the day before, with refreshments courtesy of the Sunlight Foundation.

On Friday, April 11 we are having our first edit-a-thon ever with the Library of Congress. The Africa Collection Edit-a-Thon will focus on the Library's African and Middle East Reading Room. It'll be early in the morning, but it's especially worth it if you're interested in improving Wikipedia's coverage of African topics.

The following day, we are having our second annual Wiki Loves Capitol Hill training. We will discuss policy issues relevant to Wikimedia and plan for our day of outreach to Congressional staffers that will take place during the following week.

There are other meetups in the works, so be sure to check our meetup page with the latest. I hope to see you at some of these events!

All the best, James Hare

(To unsubscribe, remove your username here.) 01:29, 26 March 2014 (UTC)

Two edit-a-thons coming up!

Hello there!

I'm pleased to tell you about two upcoming edit-a-thons:

 * This Tuesday, April 29, from 2:30 to 5:30 PM, we have the Freer and Sackler edit-a-thon. (Sorry for the short notice!)
 * On Saturday, May 10 we have the Wikipedia APA edit-a-thon, in partnership with the Smithsonian Asian Pacific American Center, from 10 AM to 5 PM.

We have more stuff coming up in May and June, so make sure to keep a watch on the DC meetup page. As always, if you have any recommendations or requests, please leave a note on the talk page.

Best,

James Hare

(To unsubscribe, remove your username here.) 20:38, 25 April 2014 (UTC)

Meet up with us

Happy May!

There are a few meetups in DC this month, including an edit-a-thon later this month. Check it out:
 * On Thursday, May 15 come to our evening WikiSalon at the Cove co-working space in Dupont Circle. If you're available Thursday evening, feel free to join us!
 * Or if you prefer a Saturday night dinner gathering, we also have our May Meetup at Capitol City Brewing Company. (Beer! Non-beer things too!)
 * You are also invited to the Federal Register edit-a-thon at the National Archives later this month.

Come one, come all!

Best,

James Hare

(To unsubscribe, remove your username here.) 20:20, 10 May 2014 (UTC)

ArbCom elections are now open!
MediaWiki message delivery (talk) 08:53, 23 November 2015 (UTC)

title: User talk:Lee Cremeans


text:
User talk:Prumpf

Hello Prumpf, welcome to Wikipedia. I hope you enjoy editing here and being a Wikipedian. You can learn more on the how to edit page. The naming conventions and manual of style pages are also useful. Feel free to experiment at the Sandbox. If you have any questions about the project then check out Help or add a question to the Village pump. Angela

Spiritus Lenis entry.
Greetings,

I am curious as to the source for the statement, 'Some think it signifies the glottal stop some languages use to avoid initial vowel sounds' in the definition of 'Spiritus Lenis'.

Thank you,

Tracey Lane tlane@kingsseminary.edu 818.779.8421

 * I couldn't find one. I think I read it in one of my Greek textbooks when I was in school, and I don't have those anymore, so it should probably be considered apocryphal information.

 * Prumpf 18:17, 28 Jun 2004 (UTC)

Bohr compactification
I reverted to what I had written earlier. The edits you made are simply not correct. I agree the article has to be a little more informative. I will try to add something useful later.

You said the canonical "Bohr" map always bijective, but need not be a homeomorphism. It certainly is injective for abelian groups, but injectivity is holds only for so-called "almost periodic groups" those which have a seprating family of finite dimensional unitary representations. non-compact semi-simple groups for instance SL(2,R) only have non-trivial representations which are infinite dimensional. CSTAR 17:14, 3 Sep 2004 (UTC)

 * Let G_ch be G with the chaotic topology (i.e. only G_ch and the empty set are open in G_ch). The identity map f: G -> G_ch is a continuous homomorphism, and G_ch is compact, so by the universal property of the Bohr compactification there is a map from βG to G_ch that's the identity on the embedded copy of G.  Thus, the map from G to βG is injective.

 * Am I still confused about this? We might want to clarify that the Bohr compactification need not be Hausdorff, but I think considering the Bohr topology as a topology on G that might just fail to be Hausdorff rather than a topology on a quotient of G that always is Hausdorff. Prumpf 17:23, 3 Sep 2004 (UTC)

 * OK, maybe one should say mappings into compact Hausdorff groups. The Bohr compactification in the sense of mappings into more general quasi-compact (i.e. compact but non-Hausdorff) topological groups is hardly useful. CSTAR 19:14, 3 Sep 2004 (UTC)

 * How is it not useful? I seem to remember it as the more popular definition and it makes more sense to me (the Bohr compactification, in my sense, is an actual compactification of a topological group that is very similar to G, but has a potentially coarser topology.  I'm rather tempted to be bold on this, at least as far as restoring some of my edit is concerned.  Prumpf 07:58, 4 Sep 2004 (UTC)

 * The Bohr compactification in the sense of being universal with respect to mappings into more general quasi-compact groups is not useful because it does not have a Haar measure! That's one of the main points of the Bohr-compactification: the mean value of almost periodic function f is exactly the integral of the extension.CSTAR 16:50, 20 Sep 2004 (UTC)

Cat:Math
I did not appreciate your reversion of Mathematical constant without explanation. I am trying to keep Cat:Math relatively free of articles and I think the articles should belong to one of Cat:Math's subcategories. If you did not like the categorization I made for the article, could you please then categorize Mathematical constant into a relevant subcategory yourself. Dysprosia 22:21, 7 Sep 2004 (UTC)

I saw the problem, sorry bout the inadvertent removal of interwiki links... Dysprosia 22:28, 7 Sep 2004 (UTC)

 * Let me explain. I did look at the diff, and it seemed to consist of two things: 1) moving the article into Category:Numbers, where it does not belong, since it's not about any number (this is my understanding of the plural naming convention for categories) 2) what appeared to be a removal of all interwiki links.  I realised I was wrong about 2) since they got duplicated beforehand, which wasn't obvious from the diff, of course, so I removed it again.

 * My apologies for reverting without explanation; as I just said, at the time it looked to me as though some of the reverted changes were borderline vandalistic.  I still don't believe the article belongs in Category:Numbers (I suppose a table of mathematical constants might go there, but an article about what mathematical constants are shouldn't).  I think the total Stiefel-Whitney class and similar constructions could reasonably be called "constants" without even being numbers.

 * So my proposal would be that Mathematical constant is a non-formalised mathematical concept, like pathological (mathematics) and well-behaved. A new category for those, maybe?

 * Again, sorry for the hasty revert. I'll try to avoid doing that in the future.

 * Prumpf 22:42, 7 Sep 2004 (UTC)

 * Argh, sorry for deleting your comment. I'm not sure how I managed that, actually, since we had an edit conflict and I didn't get a conflict warning.  Prumpf 22:45, 7 Sep 2004 (UTC)

more on Natural Units
could you take a look at my talk page? i posted a more current version of that sci.physics.research article that i called "The Most Natural Physical Units". i really believe that the Planck current is wrong on the Natural units page. but, in addition, more thought should be put into the concept of Natural Units and not simply equate them to Planck Units.

r b-j 03:29, 17 Sep 2004 (UTC)

Group algebras
Could we break up the Group ring article into two articles? (e.g. general group rings over fields and the group C*-algebra or some such division)? If you agree, would you be willing to take a crack at it or should I do it?CSTAR 16:46, 20 Sep 2004 (UTC)

 * I'm not sure whether the natural division would be "group ring" vs "group algebra (with a topology)" or group algebra of a discrete group (discrete or von Neumann) vs group algebra of a topological group. That we seem to have two definitions of the group von Neumann algebra of a discrete group now (and I don't think they coincide - unless the enveloping von Neumann algebras of the reduced group C* algebra is always isomorphic to that of the non-reduced one?) doesn't really help.

 * We really should make it very clear in the group ring article that a group ring can be considered over any ring, Z in particular. Undergraduates will most likely see group cohomology or (topological) cohomology with local coefficients at some point.

 * So, my (new) suggestion is a fairly basic article at group ring, and moving the current article to group algebra. I shall do it as soon as I'm convinced it really wouldn't be useful to treat group rings and the group C* algebra all in one article.  Feel free to be bold and make that decision for me (to criticise ;)), obviously.  Prumpf 00:22, 22 Sep 2004 (UTC)

Lens space Cat.
Hi. I was just wondering why you removed this from algebraic topology, but left it in differential such. mat_x 20:36, 28 Sep 2004 (UTC)

 * Hmm. I think it doesn't belong in category:differential topology either, but I'm not sure.  However, I don't see any connection to algebraic topology other than that lens spaces happen to be good examples for some phenomena there. Prumpf 00:28, 29 Sep 2004 (UTC)

 * I don't really know, or in fact care about, the eligability criteria for being in a category. If you think this does not warrant an entry, that's fine by me. Infinite-dimensional lens spaces are $$K(\mathbb Z_m,1)$$s though... mat_x 14:16, 29 Sep 2004 (UTC)

 * Hmm. I was just a bit worried about category:Algebraic topology growing too large, and I didn't notice that fact in the lens space article.  I suppose category:Eilenberg-MacLane spaces would be a way to deal with those articles ... Prumpf 14:35, 29 Sep 2004 (UTC)

 * I understand; I don't think anyone has got round to adding that fact yet. I certainly overlooked it when the article was created. Good suggestion though ;-$

more on Natural Units
hi Prumpf. just to let you know that there is a response to your last message on my talk page. also, my intention has been to be completely respectful and open-minded. i hope i've lived up to that and if i haven't, feel free to tell me. again, i ain't in the same league as you so, unless it's impossible, we need to make the arguments at the level of an EE grad student or a physics junior or i will likely not be able to understand it. thanks for paying attention to the issue. r b-j 00:59, 1 Oct 2004 (UTC)

oh, feel free to delete this from your talk page, i just wanted to get your attention.

 * Thanks. No need to worry, I'm just a bit busy.  I'll definitely get back to you once I've worked out what exactly happens to Maxwell's equations in my proposed unit system.  Prumpf 03:13, 1 Oct 2004 (UTC)

 * cool. our differences regarding which form of Planck's constant (with or without the 1/(2*pi)) will make no difference on Maxwell's Eqs. (but it *will* make a difference on Schrödinger's equation) but you won't get Maxwell's Eqs. (and Lorentz):

div(E) =  rho/epsilon_0         = c*Z_0*rho div(B) =  0   curl(E) = -(dB/dt)/c curl(B) = (dE/dt)/c + c*mu_0*J  = (dE/dt)/c + Z_0*J = (dE/dt)/c + Z_0*rho*velocity F = q*(E +  v/c x B)

 * as simple as:

div(E) =  rho div(B) =  0 curl(E) = -dB/dt curl(B) = dE/dt + J   =   dE/dt + rho*velocity

F = q*(E +  v x B)

 * without normalizing both epsilon_0 and mu_0 (or equivalently both c and Z_0). that means there is a 1/(4*pi*r^2) in the inverse-square laws such as Coulomb's and Newton's.

 * r b-j 03:42, 2 Oct 2004 (UTC)

 * Who says curl and div are natural? They're (usually) defined in coordinates, and in cleaner notation depend on the isomorphism of smooth functions on a manifold with volume forms, which should have an added factor of 4*pi in it somewhere.

 * My (current) idea of naturalness is to start with a natural set of measures on a (semi-)Riemannian manifold -- the Hausdorff measures will do just fine. I'm willing to accept d/dt as a natural operator, since time is special.  However, the same argument doesn't apply to d/dx aso, since that would mean choosing coordinates -- something I'm (so far) trying to avoid.

 * I haven't lost interest in this, just really haven't found the time of sitting down and making a list of all the equations we want to naturalise, and where what kind of measure/unit comes in.

 * Prumpf 18:49, 11 Oct 2004 (UTC)

Bell curve
I have redirected Bell Curve (with capital letters) to bell curve (with lower-case letters) and made the latter into a proper disambiguation page with links to normal distribution and to the book. Therefore, no one following the link to Bell Curve will find the normal distribution article and there should be no need for a notice informing the reader of the existence of a book whose title is not similar to that of the article and that has little relevance to the article's topic. Michael Hardy 23:03, 16 Nov 2004 (UTC)

Article Licensing
Hi, I've started a drive to get users to multi-license all of their contributions that they've made to either (1) all U.S. state, county, and city articles or (2) all articles, using the Creative Commons Attribution-Share Alike (CC-by-sa) v1.0 and v2.0 Licenses or into the public domain if they prefer. The CC-by-sa license is a true free documentation license that is similar to Wikipedia's license, the GFDL, but it allows other projects, such as WikiTravel, to use our articles. Since you are among the top 2000 Wikipedians by edits, I was wondering if you would be willing to multi-license all of your contributions or at minimum those on the geographic articles. Over 90% of people asked have agreed. For More Information:
 * Multi-Licensing FAQ - Lots of questions answered
 * Multi-Licensing Guide
 * Free the Rambot Articles Project

To allow us to track those users who muli-license their contributions, many users copy and paste the " " template into their user page, but there are other options at Template messages/User namespace. The following examples could also copied and pasted into your user page:

 * Option 1
 * I agree to multi-license all my contributions, with the exception of my user pages, as described below:

OR
 * Option 2
 * I agree to multi-license all my contributions to any U.S. state, county, or city article as described below:

Or if you wanted to place your work into the public domain, you could replace " " with "  ". If you only prefer using the GFDL, I would like to know that too. Please let me know what you think at my talk page. It's important to know either way so no one keeps asking. -- Ram-Man (comment| talk)

Notice
Hey. What's the deal with the ad for cafe press under the fund drive message? ISTR a policy of not running ads on wikipedia, and it's pretty annoying to boot. If there's a good reason for it (maybe cafe press is supporting us or something?), it might be a good idea to at least link to an explanation rather than just alienating random editors. It's not even entirely clear (to me) who put that message there, but your user name (Eloquence) shows up on the cafe press page.

 * Hello. This is not really an ads. The benefits of the sales get to the Wikimedia Foundation itself, and in exchange editors get nice tee-shirts, mugs etc... with the wikipedia logo on it.

 * The decision to put this comment was made by the CFO of the board, and as part of the board, I approve it. You may consider it as part of the fundraising.

 * Eloquence gets no benefit of the sales, but his name is mentionned because he nicely set that shop for the Foundation possibly a year ago.

 * Cheers. Anthere 19:12, 1 Mar 2005 (UTC) Vice-chair Wikimedia Foundation Inc.

 * Thanks for the speedy reply. I do not see how this is not an advertisement, in that it tells users to purchase products from a for-profit company.  In saying that the benefits of the sales go to the Wikimedia Foundation, are you saying that Cafe Press does not benefit from sales made through the link?

 * I did not want to imply that Eloquence profitted from the advertisement, or that it was added out of anything but the best intentions.

 * I assume that's Daniel Mayer? Thanks for telling me that, I will talk to him if this continues to be an issue.

 * Thanks again. Prumpf 19:36, 1 Mar 2005 (UTC)

tagesschau
Look to the german wikipedia and tagesschau.de. I corrected the article. The ARD tagesschau is not capitalised. --ThomasK 04:41, August 13, 2005 (UTC)

 * tagesschau.de is not. Tagesschau is.  The page title of tagesschau.de/index.html is Aktuelle Nachrichten - Inland Ausland Wirtschaft Kultur Sport  - ARD Tagesschau.  Note capitalisation. 15:32, August 21, 2005 Prumpf

You are wrong. I corrected the article, because the tagesschau of Germany (both) is not capitalised. --ThomasK 12:54, August 25, 2005 (UTC)

 * Let's move this to the proper discussion page. Prumpf 19:43, 26 August 2005 (UTC)

ArbCom elections are now open!
MediaWiki message delivery (talk) 08:53, 23 November 2015 (UTC)

title: User talk:Prumpf


text:
User talk:LeeJames~enwiki

Hello LeeJames, welcome to Wikipedia. I hope you enjoy editing here and being a Wikipedian. You can learn more on the how to edit page. The naming conventions and style guide pages are also useful. There is a sandbox which you can use to experiment in. If you have any questions, see the help pages or add a question to the village pump. Angela

Your account will be renamed
Hello,

The developer team at Wikimedia is making some changes to how accounts work, as part of our on-going efforts to provide new and better tools for our users like cross-wiki notifications. These changes will mean you have the same account name everywhere. This will let us give you new features that will help you edit and discuss better, and allow more flexible user permissions for tools. One of the side-effects of this is that user accounts will now have to be unique across all 900 Wikimedia wikis. See the announcement for more information.

Unfortunately, your account clashes with another account also called LeeJames. To make sure that both of you can use all Wikimedia projects in future, we have reserved the name LeeJames~enwiki that only you will have. If you like it, you don't have to do anything. If you do not like it, you can pick out a different name. If you think you might own all of the accounts with this name and this message is in error, please visit Special:MergeAccount to check and attach all of your accounts to prevent them from being renamed.

Your account will still work as before, and you will be credited for all your edits made so far, but you will have to use the new account name when you log in.

Sorry for the inconvenience.

Yours, Keegan Peterzell Community Liaison, Wikimedia Foundation 01:18, 20 March 2015 (UTC)

Renamed
 This account has been renamed as part of single-user login finalisation. If you own this account you can |log in using your previous username and password for more information. If you do not like this account's new name, you can choose your own using this form after logging in: . -- Keegan (WMF) (talk) 15:21, 22 April 2015 (UTC)

title: User talk:LeeJames~enwiki


text:
Astronomical spectroscopy

Astronomical spectroscopy is the study of astronomy using the techniques of spectroscopy to measure the spectrum of electromagnetic radiation, including visible light, ultraviolet, X-ray, infrared and radio waves that radiate from stars and other celestial objects. A stellar spectrum can reveal many properties of stars, such as their chemical composition, temperature, density, mass, distance and luminosity. Spectroscopy can show the velocity of motion towards or away from the observer by measuring the Doppler shift. Spectroscopy is also used to study the physical properties of many other types of celestial objects such as planets, nebulae, galaxies, and active galactic nuclei.

Background
Astronomical spectroscopy is used to measure three major bands of radiation in the electromagnetic spectrum: visible light, radio waves, and X-rays. While all spectroscopy looks at specific bands of the spectrum, different methods are required to acquire the signal depending on the frequency. Ozone (O3) and molecular oxygen (O2) absorb light with wavelengths under 300 nm, meaning that X-ray and ultraviolet spectroscopy require the use of a satellite telescope or rocket mounted detectors. Radio signals have much longer wavelengths than optical signals, and require the use of antennas or radio dishes. Infrared light is absorbed by atmospheric water and carbon dioxide, so while the equipment is similar to that used in optical spectroscopy, satellites are required to record much of the infrared spectrum.

Optical spectroscopy
Physicists have been looking at the solar spectrum since Isaac Newton first used a simple prism to observe the refractive properties of light. In the early 1800s Joseph von Fraunhofer used his skills as a glassmaker to create very pure prisms, which allowed him to observe 574 dark lines in a seemingly continuous spectrum. Soon after this, he combined telescope and prism to observe the spectrum of Venus, the Moon, Mars, and various stars such as Betelgeuse; his company continued to manufacture and sell high-quality refracting telescopes based on his original designs until its closure in 1884.

The resolution of a prism is limited by its size; a larger prism will provide a more detailed spectrum, but the increase in mass makes it unsuitable for highly detailed work. This issue was resolved in the early 1900s with the development of high-quality reflection gratings by J.S. Plaskett at the Dominion Observatory in Ottawa, Canada. Light striking a mirror will reflect at the same angle, however a small portion of the light will be refracted at a different angle; this is dependent upon the indices of refraction of the materials and the wavelength of the light. By creating a "blazed" grating which utilizes a large number of parallel mirrors, the small portion of light can be focused and visualized. These new spectroscopes were more detailed than a prism, required less light, and could be focused on a specific region of the spectrum by tilting the grating.

The limitation to a blazed grating is the width of the mirrors, which can only be ground a finite amount before focus is lost; the maximum is around 1000 lines/mm. In order to overcome this limitation holographic gratings were developed. Volume phase holographic gratings use a thin film of dichromated gelatin on a glass surface, which is subsequently exposed to a wave pattern created by an interferometer. This wave pattern sets up a reflection pattern similar to the blazed gratings but utilizing Bragg diffraction, a process where the angle of reflection is dependent on the arrangement of the atoms in the gelatin. The holographic gratings can have up to 6000 lines/mm and can be up to twice as efficient in collecting light as blazed gratings. Because they are sealed between two sheets of glass, the holographic gratings are very versatile, potentially lasting decades before needing replacement.

Light dispersed by the grating or prism in a spectrograph can be recorded by a detector. Historically, photographic plates were widely used to record spectra until electronic detectors were developed, and today optical spectrographs most often employ charge-coupled devices (CCDs). The wavelength scale of a spectrum can be calibrated by observing the spectrum of emission lines of known wavelength from a gas-discharge lamp. The flux scale of a spectrum can be calibrated as a function of wavelength by comparison with an observation of a standard star with corrections for atmospheric absorption of light; this is known as spectrophotometry.

Radio spectroscopy
Radio astronomy was founded with the work of Karl Jansky in the early 1930s, while working for Bell Labs. He built a radio antenna to look at potential sources of interference for transatlantic radio transmissions. One of the sources of noise discovered came not from Earth, but from the center of the Milky Way, in the constellation Sagittarius. In 1942, JS Hey captured the Sun's radio frequency using military radar receivers. Radio spectroscopy started with the discovery of the 21-centimeter H I line in 1951.

Radio interferometry
Radio interferometry was pioneered in 1946, when Joseph Lade Pawsey, Ruby Payne-Scott and Lindsay McCready used a single antenna atop a sea cliff to observe 200 MHz solar radiation. Two incident beams, one directly from the sun and the other reflected from the sea surface, generated the necessary interference. The first multi-receiver interferometer was built in the same year by Martin Ryle and Vonberg. In 1960, Ryle and Antony Hewish published the technique of aperture synthesis to analyze interferometer data. The aperture synthesis process, which involves autocorrelating and discrete Fourier transforming the incoming signal, recovers both the spatial and frequency variation in flux. The result is a 3D image whose third axis is frequency. For this work, Ryle and Hewish were jointly awarded the 1974 Nobel Prize in Physics.

Chemical properties
Newton used a prism to split white light into a spectrum of color, and Fraunhofer's high-quality prisms allowed scientists to see dark lines of an unknown origin. In the 1850s, Gustav Kirchhoff and Robert Bunsen described the phenomena behind these dark lines. Hot solid objects produce light with a continuous spectrum, hot gases emit light at specific wavelengths, and hot solid objects surrounded by cooler gases show a near-continuous spectrum with dark lines corresponding to the emission lines of the gases. By comparing the absorption lines of the Sun with emission spectra of known gases, the chemical composition of stars can be determined.

The major Fraunhofer lines, and the elements with which they are associated, appear in the following table. Designations from the early Balmer Series are shown in parentheses.

Not all of the elements in the Sun were immediately identified. Two examples are listed below: To date more than 20 000 absorption lines have been listed for the Sun between 293.5 and 877.0 nm, yet only approximately 75% of these lines have been linked to elemental absorption.
 * In 1868 Norman Lockyer and Pierre Janssen independently observed a line next to the sodium doublet (D1 and D2) which Lockyer determined to be a new element. He named it Helium, but it wasn't until 1895 the element was found on Earth.
 * In 1869 the astronomers Charles Augustus Young and William Harkness independently observed a novel green emission line in the Sun's corona during an eclipse. This "new" element was incorrectly named coronium, as it was only found in the corona. It was not until the 1930s that Walter Grotrian and Bengt Edlén discovered that the spectral line at 530.3 nm was due to highly ionized iron (Fe13+). Other unusual lines in the coronal spectrum are also caused by highly charged ions, such as nickel and calcium, the high ionization being due to the extreme temperature of the solar corona.

By analyzing the equivalent width of each spectral line in an emission spectrum, both the elements present in a star and their relative abundances can be determined. Using this information stars can be categorized into stellar populations; Population I stars are the youngest stars and have the highest metal content (the Sun is a Pop I star), while Population III stars are the oldest stars with a very low metal content.

Temperature and size
In 1860 Gustav Kirchhoff proposed the idea of a black body, a material that emits electromagnetic radiation at all wavelengths. In 1894 Wilhelm Wien derived an expression relating the temperature (T) of a black body to its peak emission wavelength (λmax):

b is a constant of proportionality called Wien's displacement constant, equal to This equation is called Wien's Law. By measuring the peak wavelength of a star, the surface temperature can be determined. For example, if the peak wavelength of a star is 502 nm the corresponding temperature will be 5772 kelvins.

The luminosity of a star is a measure of the electromagnetic energy output in a given amount of time. Luminosity (L) can be related to the temperature (T) of a star by:

where R is the radius of the star and σ is the Stefan–Boltzmann constant, with a value of Thus, when both luminosity and temperature are known (via direct measurement and calculation) the radius of a star can be determined.

Galaxies
The spectra of galaxies look similar to stellar spectra, as they consist of the combined light of billions of stars.

Doppler shift studies of galaxy clusters by Fritz Zwicky in 1937 found that the galaxies in a cluster were moving much faster than seemed to be possible from the mass of the cluster inferred from the visible light. Zwicky hypothesized that there must be a great deal of non-luminous matter in the galaxy clusters, which became known as dark matter. Since his discovery, astronomers have determined that a large portion of galaxies (and most of the universe) is made up of dark matter. In 2003, however, four galaxies (NGC 821, NGC 3379, NGC 4494, and NGC 4697) were found to have little to no dark matter influencing the motion of the stars contained within them; the reason behind the lack of dark matter is unknown.

In the 1950s, strong radio sources were found to be associated with very dim, very red objects. When the first spectrum of one of these objects was taken there were absorption lines at wavelengths where none were expected. It was soon realised that what was observed was a normal galactic spectrum, but highly red shifted. These were named quasi-stellar radio sources, or quasars, by Hong-Yee Chiu in 1964. Quasars are now thought to be galaxies formed in the early years of our universe, with their extreme energy output powered by super-massive black holes.

The properties of a galaxy can also be determined by analyzing the stars found within them. NGC 4550, a galaxy in the Virgo Cluster, has a large portion of its stars rotating in the opposite direction as the other portion. It is believed that the galaxy is the combination of two smaller galaxies that were rotating in opposite directions to each other. Bright stars in galaxies can also help determine the distance to a galaxy, which may be a more accurate method than parallax or standard candles.

Interstellar medium
The interstellar medium is matter that occupies the space between star systems in a galaxy. 99% of this matter is gaseous – hydrogen, helium, and smaller quantities of other ionized elements such as oxygen. The other 1% is dust particles, thought to be mainly graphite, silicates, and ices. Clouds of the dust and gas are referred to as nebulae.

There are three main types of nebula: absorption, reflection, and emission nebulae. Absorption (or dark) nebulae are made of dust and gas in such quantities that they obscure the starlight behind them, making photometry difficult. Reflection nebulae, as their name suggest, reflect the light of nearby stars. Their spectra are the same as the stars surrounding them, though the light is bluer; shorter wavelengths scatter better than longer wavelengths. Emission nebulae emit light at specific wavelengths depending on their chemical composition.

Gaseous emission nebulae
In the early years of astronomical spectroscopy, scientists were puzzled by the spectrum of gaseous nebulae. In 1864 William Huggins noticed that many nebulae showed only emission lines rather than a full spectrum like stars. From the work of Kirchhoff, he concluded that nebulae must contain "enormous masses of luminous gas or vapour." However, there were several emission lines that could not be linked to any terrestrial element, brightest among them lines at 495.9 nm and 500.7 nm. These lines were attributed to a new element, nebulium, until Ira Bowen determined in 1927 that the emission lines were from highly ionised oxygen (O+2). These emission lines could not be replicated in a laboratory because they are forbidden lines; the low density of a nebula (one atom per cubic centimetre) allows for metastable ions to decay via forbidden line emission rather than collisions with other atoms.

Not all emission nebulae are found around or near stars where solar heating causes ionisation. The majority of gaseous emission nebulae are formed of neutral hydrogen. In the ground state neutral hydrogen has two possible spin states: the electron has either the same spin or the opposite spin of the proton. When the atom transitions between these two states, it releases an emission or absorption line of 21 cm. This line is within the radio range and allows for very precise measurements: Using this information, the shape of the Milky Way has been determined to be a spiral galaxy, though the exact number and position of the spiral arms is the subject of ongoing research.
 * Velocity of the cloud can be measured via Doppler shift
 * The intensity of the 21 cm line gives the density and number of atoms in the cloud
 * The temperature of the cloud can be calculated

Complex molecules
Dust and molecules in the interstellar medium not only obscures photometry, but also causes absorption lines in spectroscopy. Their spectral features are generated by transitions of component electrons between different energy levels, or by rotational or vibrational spectra. Detection usually occurs in radio, microwave, or infrared portions of the spectrum. The chemical reactions that form these molecules can happen in cold, diffuse clouds or in dense regions illuminated with ultraviolet light. Most known compounds in space are organic, ranging from small molecules e.g. acetylene C2H2 and acetone (CH3)2CO; to entire classes of large molecule e.g. fullerenes and polycyclic aromatic hydrocarbons; to solids, such as graphite or other sooty material.

Motion in the universe
Stars and interstellar gas are bound by gravity to form galaxies, and groups of galaxies can be bound by gravity in galaxy clusters. With the exception of stars in the Milky Way and the galaxies in the Local Group, almost all galaxies are moving away from Earth due to the expansion of the universe.

Doppler effect and redshift
The motion of stellar objects can be determined by looking at their spectrum. Because of the Doppler effect, objects moving towards someone are blueshifted, and objects moving away are redshifted. The wavelength of redshifted light is longer, appearing redder than the source. Conversely, the wavelength of blueshifted light is shorter, appearing bluer than the source light:
 * $$\frac{\lambda-\lambda_0}{\lambda_0}=\frac{v_0}{c}$$

where $$\lambda_0$$ is the emitted wavelength, $$v_0$$ is the velocity of the object, and $$\lambda$$ is the observed wavelength. Note that v<0 corresponds to λ<λ0, a blueshifted wavelength. A redshifted absorption or emission line will appear more towards the red end of the spectrum than a stationary line. In 1913 Vesto Slipher determined the Andromeda Galaxy was blueshifted, meaning it was moving towards the Milky Way. He recorded the spectra of 20 other galaxies — all but four of which were redshifted — and was able to calculate their velocities relative to the Earth. Edwin Hubble would later use this information, as well as his own observations, to define Hubble's law: The further a galaxy is from the Earth, the faster it is moving away. Hubble's law can be generalised to:
 * $$v = H_0 d$$

where $$v$$ is the velocity (or Hubble Flow), $$H_0$$ is the Hubble Constant, and $$d$$ is the distance from Earth.

Redshift (z) can be expressed by the following equations:

In these equations, frequency is denoted by $$f$$ and wavelength by $$\lambda$$. The larger the value of z, the more redshifted the light and the farther away the object is from the Earth. As of January 2013, the largest galaxy redshift of z~12 was found using the Hubble Ultra-Deep Field, corresponding to an age of over 13 billion years (the universe is approximately 13.82 billion years old).

The Doppler effect and Hubble's law can be combined to form the equation $$z = \frac{v_\text{Hubble}}{c}$$, where c is the speed of light.

Peculiar motion
Objects that are gravitationally bound will rotate around a common center of mass. For stellar bodies, this motion is known as peculiar velocity and can alter the Hubble Flow. Thus, an extra term for the peculiar motion needs to be added to Hubble's law:
 * $$v_\text{total} = H_0 d + v_\mathrm{pec}$$

This motion can cause confusion when looking at a solar or galactic spectrum, because the expected redshift based on the simple Hubble law will be obscured by the peculiar motion. For example, the shape and size of the Virgo Cluster has been a matter of great scientific scrutiny due to the very large peculiar velocities of the galaxies in the cluster.

Binary stars
Just as planets can be gravitationally bound to stars, pairs of stars can orbit each other. Some binary stars are visual binaries, meaning they can be observed orbiting each other through a telescope. Some binary stars, however, are too close together to be resolved. These two stars, when viewed through a spectrometer, will show a composite spectrum: the spectrum of each star will be added together. This composite spectrum becomes easier to detect when the stars are of similar luminosity and of different spectral class.

Spectroscopic binaries can be also detected due to their radial velocity; as they orbit around each other one star may be moving towards the Earth whilst the other moves away, causing a Doppler shift in the composite spectrum. The orbital plane of the system determines the magnitude of the observed shift: if the observer is looking perpendicular to the orbital plane there will be no observed radial velocity. For example, a person looking at a carousel from the side will see the animals moving toward and away from them, whereas if they look from directly above they will only be moving in the horizontal plane.

Planets, asteroids, and comets
Planets, asteroids, and comets all reflect light from their parent stars and emit their own light. For cooler objects, including Solar System planets and asteroids, most of the emission is at infrared wavelengths we cannot see, but that are routinely measured with spectrometers. For objects surrounded by gas, such as comets and planets with atmospheres, further emission and absorption happens at specific wavelengths in the gas, imprinting the spectrum of the gas on that of the solid object. In the case of worlds with thick atmospheres or complete cloud or haze cover (such as the four giant planets, Venus, and Saturn's satellite Titan), the spectrum is mostly or completely due to the atmosphere alone.

Planets
The reflected light of a planet contains absorption bands due to minerals in the rocks present for rocky bodies, or due to the elements and molecules present in the atmosphere. To date over 3,500 exoplanets have been discovered. These include so-called Hot Jupiters, as well as Earth-like planets. Using spectroscopy, compounds such as alkali metals, water vapor, carbon monoxide, carbon dioxide, and methane have all been discovered.

Asteroids
Asteroids can be classified into three major types according to their spectra. The original categories were created by Clark R. Chapman, David Morrison, and Ben Zellner in 1975, and further expanded by David J. Tholen in 1984. In what is now known as the Tholen classification, the C-types are made of carbonaceous material, S-types consist mainly of silicates, and X-types are 'metallic'. There are other classifications for unusual asteroids. C- and S-type asteroids are the most common asteroids. In 2002 the Tholen classification was further "evolved" into the SMASS classification, expanding the number of categories from 14 to 26 to account for more precise spectroscopic analysis of the asteroids.

Comets
The spectra of comets consist of a reflected solar spectrum from the dusty clouds surrounding the comet, as well as emission lines from gaseous atoms and molecules excited to fluorescence by sunlight and/or chemical reactions. For example, the chemical composition of Comet ISON was determined by spectroscopy due to the prominent emission lines of cyanogen (CN), as well as two- and three-carbon atoms (C2 and C3). Nearby comets can even be seen in X-ray as solar wind ions flying to the coma are neutralized. The cometary X-ray spectra therefore reflect the state of the solar wind rather than that of the comet.

title: Astronomical spectroscopy


text:
American-born Chinese

American-born Chinese (sometimes abbreviated as ABC) is a term widely used to refer to Chinese people who were born in the United States and received U.S. citizenship due to birthright citizenship in the United States.

Contested usage
In comparison to the term Chinese American, American-born Chinese may not always denote U.S. citizenship, (mainland) Chinese nationals that were born in the United States often renounce their U.S. citizenship due to China prohibiting its citizens from holding multiple citizenships. According to some, the term has perpetual foreigner connotations. It has been noted that the term differs from existing patterns of immigrant designation in American English. For example, Peter Thiel is considered a "German-born American," and Elon Musk is considered a "South African-born Canadian-American." In both of these cases, the first demographic word refers to the person's citizenship at birth, and the second refers to his citizenship at present. However, in the case of "American-born Chinese," the first demographic word refers to the subject's citizenship at birth (or at present) and the second word to ethnicity.

It has also been observed that, in practice, the term American-born Chinese includes hundreds of thousands of Americans of Chinese descent who were, technically speaking, not born in America, but rather, were brought over by their parents at a young age. This indicates that the term may be a misnomer.

Demographics
In differing degrees, many ABCs draw together Chinese family culture with American societal culture, developing a transnational life and identity. However, this begins to shift in subsequent generations as families structures change through interracial marriage. In 2000, approximately 45% of American-born Chinese marry non-Chinese Americans; this is contrasted with Chinese Americans more generally, whereby 81.5% of men and 77.9% of women married other Chinese Americans.

In popular culture
The term was used in the 2006 graphic novel by Gene Luen Yang, entitled American Born Chinese. The book was adapted into the series of the same name for Disney+.

The term was used in the book Crazy Rich Asians, by Kevin Kwan, which has been adapted into a movie of the same name.

title: American-born Chinese


text:
User:Rednblu/CensorshipOnWikipedia

Below is a convenient workspace since a link to it appears on each Wikipedia "page"

The ban Paektu system
Interesting! There IS a system here. And that system page needs upgrading.

What element of reality does P represent that the system is unwilling to face?

P brings in incendiary material. The incendiary aspect for the W environment manifests as
 * vandalism
 * copyright
 * POV

The system will deal with the incendiary aspect by the mechanisms that the W system has for avoiding the work in the area to which the incendiary module maps.

The adaptive work for the W system is to discover how to channel P into a productive mode. An analogy might be the committed Christian. How do you get the Christian into productive mode dealing with reality?
 * As a model of the interaction of the system components, the Christian model might be useful. The OS has various methods of pushing the Christians into churches to keep the incendiary aspect in a safe place.
 * The al-Queda model. The OS sees no value to the al-Queda doings.
 * For example, there is the Jon David analogy. What can I do?

A for the outer system (OS)

 * Stalin and Hussein represent an opposition to the flaws of capitalism
 * S and H lose credibility because of their incendiary aspects which include:
 * brutality
 * alpha process

Questions for P

 * What is the value in what S and H represent?

Challenges in asking those questions

 * How to keep the spotlight off P
 * How to get P to use himself as data without putting himself on the cross

Questions for R
Can the W system absorb an adaptive view?

Raw data of the system workings

 * Paektu
 * Paektu/ban
 * Maveric149
 * Paektu Contributions

User:Rednblu/DevelopmentPage3...Alphabetical listing...User:Rednblu/Development/Creationism

title: User:Rednblu/CensorshipOnWikipedia


text:
Talk:Photometry (astronomy)

Name change
I removed the stellar, because spectrophometry is used for things other than stars. Most notably active galactic nuclei.

Your latest change was acceptable, the best way to solve edit conflicts is to address particularly why you are making the change - and then, rather than reverting, make an edit. Pizza Puzzle

Additions
Some content about photometric standard stars may be of interest. Praemonitus (talk) 18:33, 6 August 2018 (UTC)

New Bold Attempt and Significant Update
I have just made an bold update, improving and extending the Introduction and Methods. I've have fixed various broken or added new citations and links. New errors may have been accidental introduced and may need corrections.

The Sections under CCD photometry have no cites and seem too complex for this article. I have removed the more citation tag, and will add it to this later section. An article on photometric magnitudes need to be created and link across several dozen article on astronomical related subjects - especially on magnitude. Arianewiki1 (talk) 04:13, 20 May 2019 (UTC)

 * I have added a further update and have placed more citations supporting the article text. Lithopsian comment on original research on the 'Magnitude and colour indices is well taken, and I have added to necessary cites supporting the statement. I feel this section is important as it relates photometry to Magnitude (astronomy), apparent magnitude and absolute magnitude (which are poorly cited) and show the relationship of stellar evolution and basic or fundamental astrophysics.

 * Again. New errors may have been accidental introduced and may need corrections.

 * Related Comments
 * There is a lack of information on visual or photographic methods in this article. e,g. Using a light to project an artificial “star” into a telescope's field of view and adjusting it to match real stars in brightness or black and white filter photography with, say microdensitometers), which pertains to 'photometry' and links visual observations to electronic photometry (including magnitude systems.) Once accepted, some of this text might be applied to these other magnitude related pages in some form.

 * There also needs some comments on measuring the surface brightness of planets and deep-sky objects.

 * The section on 'CCD photometry' could be place as a new article or placed under 'Charge-coupled device' say Section 'Use in astronomy.' (There is no mention of CCD photometry in that section.) As the article is at present, most of this section's text could be rightfully removed, especially with the lack of citations. I have prepared an rough draft example in my Arianewiki1 sandbox. Any opinions or advice to formally do this? Arianewiki1 (talk) 03:53, 22 May 2019 (UTC)

 * Hello- You suggested that an article needs to be created on "photometric magnitudes". I don't think that this is necessary at all: there are already articles on Magnitude (astronomy), Apparent magnitude, Absolute magnitude, and photometry, and the term "photometric magnitudes" isn't a thing that requires an article separate from these ones that already exist. I also don't think there's any need for a separate article on "CCD photometry". The photometry article seems like the appropriate place to explain that most visible wavelength photometry is done using CCD cameras and give some information about that, which the article already does. Also: I noticed that some of the newly added text in the article says that magnitudes measured using photometers are denoted with capital letters, but that isn't correct: magnitudes are designated by the filter name which can be upper or lower case depending on the filter set. Aldebarium (talk) 00:00, 23 May 2019 (UTC)
 * Thanks for your patience while I've being trying to improving this article page.
 * After doing this, I agree that "photometric magnitudes" might not need an additional article, though it might be perhaps be better defined in the Magnitude (astronomy) article?
 * The problem I see with the CCD photometry section is more technical with operational aspects of using CCD electronics than photometry issues. I needs a expert to write and cite this additional text, which needs a lot of work to be relevant. There needs to be information about amateur CCD photometry (which the section is mostly about): but also lacking professional and satellite photometric methods.
 * The last point on photometric filters is well taken. The statement is true with UBV photometry versus visual or photographic methods, but isn't true when considering other photometric systems. The last paragraph says: "Due to the large number of different photometric systems adopted by astronomers, there are many expressions of magnitudes and their indices. Each system assigns an upper or lower case letter to the filter used."
 * I've looked more closely at the text and have modify these statements accordingly. (This applies to the older UBV, UBVRI or JHK systems, but not to the newer systems.) Arianewiki1 (talk) 04:39, 23 May 2019 (UTC)

CCD subsections
Are all these methods (absolute, differential, surface, forced, etc) really part of CCD only? Jim.henderson (talk) 11:47, 24 May 2023 (UTC)

 * No. The techniques can be used with any imaging detector or with a simple aperture photometer. It's odd that they are currently discuessed within the CCD section when they are general techniques. TowardsTheLight (talk) 12:35, 24 May 2023 (UTC)

title: Talk:Photometry (astronomy)