Einstein@home, Поиск нейтронных звезд, излучающих гравитационные волны Налаштування

[Panda]

Проект "Einstein@home"

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Официальный сайт
Статистика по команде "Ukraine"
Статистика Free-DC
Статистика Ukraine on Free-DC

Форум команды Ukraine на сайте Einstein@Home

Состояние серверов

ТОП-20 участников:

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Дата основания команды - 08.11.2004 Капитан - Death
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Для присоединения к команде Украины:
1. Загрузите BOINC менеджер (Если его у Вас еще нет!)
2. Перейдите в "расширенный вид"
3. Выберите сервис ---> добавить проект
4. Введите адрес проекта http://einstein.phys.uwm.edu/
5. Введите свои регистрационные данные.
6. Найдите нашу команду. Она называется Ukraine и адрес ее статистики вы могли видеть выше.
7. Если есть доступные для загрузки задания Вы их получите и начнете расчеты.
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Полезная информация:
Для идентификации пользователя в BOINC могут служить 2 вещи:
1) пара e-mail/пароль
2) межпроектный идентификационный ID (Cross-project ID) - 32значное шестнадцатиричное число.

Если Вы пожелаете подключится ещё и к другому BOINC-проекту, то помните: чтобы не плодить новых аккаунтов при подключении к новому проекту или команде, нужно обязательно везде регистрироваться с одним и тем же e-mail/паролем либо CPID. если при регистрации в проекте указать другие e-mail или пароль, BOINC создаст новый аккаунт с тем же именем!
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Если у вас есть желание помочь команде, не набирая очки на свою статистику, можно использовать так называемый "слабый ключ аккаунта" (weak account key) который позволяет коннектиться к проекту не вводя пароли. Все очки будут присваиваться командному юзеру distributed.org.ua

Чтобы подключиться:
0) установите BOINC
1) создайте файл account_einstein.phys.uwm.edu.xml в папке \data\
2) в файл поместите текст

<account>
    <master_url>http://einstein.phys.uwm.edu/</master_url>
    <authenticator>502209_915a010e79898a30a26f5ca74bc16437</authenticator>
    <project_name>Einstein@home</project_name>
</account>

3) перезагрузите BOINC
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О чем проект:
Einstein@Home - это проект разработанный для поиска сигналов, приходящих к нам от чрезвычайно плотных и быстровращающихся звёзд, среди данных, получаемых с Лазерного Интерферометра Обсерватории Гравитационных волн (Laser Interferometer Gravitational wave Observatory - LIGO) в США и обсерватории для поиска гравитационных волн GEO 600, расположенной в Германии. Как предполагается, их источниками могут быть кварковые и нейтронные звёзды, некоторые подклассы которых уже наблюдаются обычными средствами как пульсары или небесные объекты, излучающие в рентгеновском диапазоне. Учёные надеются, что некоторые из этих компактных звёзд могут быть не идеально сферическими, и, в таком случае, будут излучать гравитационные волны, которые смогли бы обнаружить GEO 600 и LIGO.

Галактика пролетает мимо черной дыры:


В Einstein@Home есть три вида поиска:
Gravitational Wave Search - прямой поиск гравитационных волн и самих пульсаров в данных Лазерно-интерферометрической гравитационно-волновой обсерватории (LIGO);
Gamma-ray pulsar search - поиск гамма-пульсаров в данных космической лаборатории Fermi;
Binary Radio Pulsar Search - поиск двойных радиопульсаров в данных из обсерватории в Аресибо и Паркс.

По состоянию на 24 марта 2016 года в нём приняли участие 427 535 пользователей с заработанными очками (7 217 684 компьютеров) из 222 стран.
Суммарная мощность проекта по состоянию на март 2016 г. составила свыше 2 Petaflop.
Общее количество открытых радиопульсаров — 51(июнь 2014). Добровольцы, чьи компьютеры участвовали в открытии пульсаров, получают от организаторов проекта памятный сертификат.

Открытые пульсары:

2010 год
12 августа открыт одиночный радиопульсар PSR J2007+2722.

2011 год
Открыты 15 радиопульсаров (PSR J1952+2630 в двойной звёздной системе, PSR J1322-6321, PSR J1817-1937, PSR J1840-0644, PSR J1455-5922, PSR J1644-4409, PSR J1755-3331, PSR J1619-4202, PSR J1811-1047, PSR J1838-1848, PSR J1821-0325, PSR J1950+24, PSR J1952+25, PSR J1910+10, PSR J1907+05).

2012 год
Открыты 30 радиопульсаров (PSR J1913+10, PSR J1914+14, PSR J1922+11, PSR J2005+26, PSR J2005+26, PSR J1907+09, PSR J1913+11, PSR J1858+0319, PSR J1227-6210, PSR J1601-5023, PSR J1726-3156, PSR J1855+03, PSR J1857+0259, PSR J1901+0510, PSR J1851+02, PSR J1900+0439, PSR J1953+24, PSR J1305-66, PSR J1637-46, PSR J1652-48, PSR J1838-01, PSR J0811-38, PSR J1750-25, PSR J1858-07, PSR J1748-30, PSR J1626-44, PSR J1644-46, PSR J1908+0831, PSR J1903+06, PSR J1912+09).

2013 год
Открыт 1 радиопульсар (PSR J1859+03) и 4 гамма-пульсара (PSR J0554+3107, PSR J1422-6138, PSR J1522-5735, PSR J1932+1916).

Статистика по GPU
На 24 марта 2016г.

Hosts w/ ATI/AMD GPU 6 137
Hosts w/ NVIDIA GPU 12 860
Hosts w/ INTEL HD GPU 6 550

Подробнее о проекте
Einstein@Home FAQ
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Статьи по теме:
Einstein2005
Итоги обработки данных LIGO S3 в проекте Einstein@Home
Сеть распределённых вычислений Einstein@Home насчитывает уже более 50000 пользователей
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Таблица PPD по процессорам

Процессор	Частота, GHz	Приложение	Время на задание, чч:мм	Очки
Phenom II X4 840	3.36	Gamma-ray pulsar search #2 v1.04	2:30	80
Phenom II X4 840	3.36	Gravitational Wave S6 LineVeto search (extended) v1.04 (SSE2)	06:00	250
Phenom II X4 840	3.5	Binary Radio Pulsar Search (Arecibo) v1.33 (BRP4X64)	2:13	62,5
Phenom II X4 840	3.5	Gamma-ray pulsar search #2 v1.10	23:00	880
Phenom II X4 840	3.5	Gravitational Wave S6 Directed Search (CasA) v1.05 (SSE2)	15:20	390
ARMv7 Processor rev 2 (v7l)	1	Binary Radio Pulsar Search (Arecibo) v1.43 (NEON)	28:35	62,5
Phenom II X4 840	3.5	Gamma-ray pulsar search #4 v1.04 (FGRP4-SSE2)	15:15	693
Phenom II X4 840	3.5	Gravitational Wave search S6Bucket Follow-up #2 v1.01 (SSE2)	09:12	472.85
Intel® Xeon® CPU E5430	3.2	Gravitational Wave search S6Bucket Follow-up #2 v1.01 (SSE2)	08:00	464.63
Intel® Xeon® CPU E5430	3.3	Gravitational Wave search O1 all-sky I v1.04 (X64O1I) windows_x86_64	13:30	2000
Phenom II X4 840	3.5	Gravitational Wave search O1 all-sky I v1.04 (X64O1I) windows_x86_64	33:15	2000

Примечание к таблице: указано среднее время просчета заданий. Может незначительно изменяться в обе стороны в пределах 10%.

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Важно!
Для редактирования в Вашей учетной записи настроек для карт AMD, необходимо выбрать английский язык на этой странице:
http://einstein.phys.uwm.edu/language_select.php

Статус сервера выдачи заданий:

http://www.boinc-af.org/content/view/528/156/
http://www.ligo.caltech.edu/docs/G/G060493-01/G060493-01.pdf
http://www.boinc-af.org/content/view/27/214/
http://faq.boinc.de/index.php?title=Einstein%40home
http://www.dp.by/wiki/Projects/Einsteinathome
http://www.boinc-af.org/content/view/1018/216/
http://www.boinc-af.org/content/view/1035/216/

http://wiki.bc-team.org/index.php?title=Ibercivis/en

http://wiki.bc-team.org/index.php?title=Einstein%40home/en

http://www.irelandboinc.com/projects/40-pr...95-einsteinhome
http://www.boinc.ru/Doc/Einst/einstein2005.html
http://www.boinc.ru/Doc/S3summary/s3summary.html
http://www.boinc.ru/Doc/Einst/faq_einst.htm

Це повідомлення відредагував gladiator_maximus: Mar 24 2016, 18:17

[Rilian]

Dear Einstein@Home volunteers,

the five-year upgrade of the LIGO detectors has been completed and we
are a large step closer to the first direct detection of gravitational
waves, which will mark the beginning of a new era of astronomy. As we
are writing this newsletter, Advanced LIGO is beginning its first
observation run “O1” after an extensive comissioning phase and a
series of “engineering runs”. The Einstein@Home team is truly excited
and is looking forward to the most sensitive gravitational-wave data
ever recorded.

In the first week of September more than 200 gravitational-wave
scientists from the LIGO Virgo Scientific Collaboration gathered in
Budapest for their fall meeting. Many Einstein@Home team members were
present and reported on their ongoing gravitational-wave
searches. During the meeting, the seventh issue of the LIGO Magazine
was published, featuring a four page article on Einstein@Home. You can
read it for free at [1].

Our second newsletter this year features news from the project
administration and updates from our three searches for rapidly
rotating neutron stars (through gravitational waves, radio waves, and
gamma rays). We are very happy to report three new discoveries! One
was made in data from NASA's Fermi Gamma-ray Space Telescope, and
three were made in data from the Arecibo Radio Telescope. See below
for more details on the discoveries.

Note that we are advertising a position for an Einstein@Home
computational scientist at UWM in Milwaukee [2]. If you have the
required skills and interest, please apply!

Bruce Allen, Director, Einstein@Home


News on the gravitational-wave search (M. Alessandra Papa)
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The Einstein@Home all-sky search for continuous gravitational wave
signals in the gravitational-wave frequency range from 50 Hertz to 510
Hertz is in its final stages. Thanks to your continued support we had
enough processing power to implement a hierarchy of follow-ups. Each
step was more sensitive than the previous one and would zoom in to a
signal, if present, and discard, at each step, more and more false
alarms (random fluctuations of noise mimicking a signal).

At the time of the first newsletter we were completing the first
follow-up (FU1), which looked at a total of 16 million candidates. Out
of these, the next stage (FU2) followed up about 5.5 million, using a
different set-up to increase the sensitivity. The data were split into
40 segments, each with a longer coherent observation time, namely 140
hours versus the 60 hours used in FU1. About one in every five
candidates that was looked at with FU2 was deemed worthy of being
further inspected with the third follow-up stage (FU3).

The third and final stage uses data segments of 140 hours coherent
observation time (like FU2) but with a much finer grid in parameter
space, again zooming in and increasing the sensitivity. According to
our studies, this should give us at least a 40% increase in
signal-to-noise ratio. This is sufficient to confidently separate a
possible signal from the background. In fact we expect to have no more
than a few candidates coming out of FU3, which could be confirmed or
discarded based on specific candidate-tailored studies.

FU3 is a short run, of order a few weeks, and ended in late
September. If we see something it will be extremely exciting! If we do
not, we will be able to set the most constraining upper limit on the
amplitude of continuous gravitational waves ever. And finally, the
upgraded and more sensitive Advanced LIGO detectors are coming online
these days, and we cannot wait to look at this new data.


News on the binary radio pulsar search (Benjamin Knispel)
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Our currently most active radio pulsar search is a more sensitive
re-analysis of the Parkes Multi-beam Pulsar Survey (PMPS). It covers a
larger parameter space than analyzed in a previous Einstein@Home
search of the same data set. Since the start in March we have
processed roughly 30% of all observations. So far no new discoveries
have been made, but we have seen some interesting candidates and
re-discovered many known pulsars.

Whenever we get ‘fresh’ data from the PALFA survey with the Arecibo
telescope, we sent them out to your GPUs and Android devices
immediately. Over the past months we received four batches of new
data. In the latest data, we have made new radio pulsar
discoveries. Three of them (J1955+29, J1853+00, and J1853+0029) have
already been confirmed by the required follow-up observation. Congrats
to Przemek Wisialski and Gary S. Grant II, robert dolezal and Jim
Trettel, and [TiDC] Chulma - S'inergy and boinc_qc whose computers
found the pulsars with the highest statistical significance! The
follow-up observations for one remaining candidate will be done soon
with the Arecibo radio telescope.

Finally, a paper reporting on an earlier Einstein@Home radio pulsar
discovery in PALFA data has been published in The Astrophysical
Journal [3]. You can read it for free on the arXiv preprint server
[4]. The paper presents the discovery of a millisecond pulsar in a
surprisingly eccentric orbit, and looks at how this system and the
four known similar ones might have formed. In any case, they cannot
have formed through what has been thought to be the standard way of
making millisecond pulsars, i.e., through spinning up an older pulsar
by transfer of matter from a companion star. You can read more
background info at [5].


News on the gamma-ray pulsar search (Holger Pletsch)
----------------------------------------------------
The various improvements offered by the latest, still ongoing, survey
of unidentified gamma-ray sources have borne first fruit. Earlier this
month we announced the Einstein@Home discovery of a new gamma-ray
pulsar hidden in plain sight in data from the Fermi Gamma-ray Space
Telescope, which has been published in the Astrophysical Journal
Letters [6] (open-access preprint available at [7], accompanying press
release at [8]). Further exciting candidate discoveries are currently
being studied in detail. We also examining the feasibility of
expanding the survey to other pulsar system types not yet searched on
Einstein@Home.


News from the project administration (Bernd Machenschalk)
---------------------------------------------------------
For the gamma-ray pulsar search we issued new application versions
that include a minor bug fix (typo in numerical constant) and feature
checkpointing during the last (“follow-up”) stage of a task, which was
previously not interruptable. This allows us to now slightly increase
the number of follow-up candidates to squeeze the last bit of
sensitivity out of the computation.

The “S6Bucket Follow-Up run #2” has ended (see above) and the third
stage of the follow-up will run until the end of September. After the
end of the third stage, there will be no new gravitational-wave search
for a while, and the project's CPUs will run 100% gamma-ray pulsar
search.

The binary radio pulsar search applications have been updated as well:
Optimizations that mainly reduce the amount of data that needs to be
shifted between GPU and CPU memory were implemented for both BRP4
(Arecibo data) and BRP6 (Barkes data), in application versions
1.52. The optimizations resulted in a speedup of up to 50%. There are
also CUDA application versions currently in Beta test with an updated
version of CUDA (5.5 instead of previously used 3.2). The speedup
gained from using these versions highly depends on the card used, it
varies between zero and another 50%.

For the general server infrastructure we performed additional numerous
system software and security updates, and am in the process of
replacing old servers that have become unreliable by modern hardware.

[1] http://www.ligo.org/magazine/LIGO-magazine...e-7.pdf#page=18
[2] http://jobs.uwm.edu/postings/23976
[3] http://iopscience.iop.org/0004-637X/806/1/140/
[4] http://arxiv.org/abs/1504.03684
[5] http://einstein.phys.uwm.edu/forum_thread.php?id=11257
[6] http://iopscience.iop.org/2041-8205/809/1/L2/
[7] http://arxiv.org/abs/1508.00779/
[8] http://www.aei.mpg.de/1689618/EatHGPSRHidden

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If you would like to discuss this newsletter with other Einstein@Home
volunteers, and the project developers and scientists, please visit
this thread in the discussions forum:
http://einstein.phys.uwm.edu/forum_thread.php?id=11499


Thank you for your continued support, Bruce Allen, Benjamin Knispel,
Bernd Machenschalk, M. Alessandra Papa, and Holger Pletsch for the
Einstein@Home team