
Arabic: 
ترجمة: علي إبراهيم Ali M Ibrahem
 
Twitter:@96_alimibra
لسنوات إستطاع علماء الفلك
أن يجدوا إلى ما يصل إلى نصف المادة في الكون
مشكلة المادة الباريونيّة المفقودة وضعت فهمنا لفيزياء الإنفجار العظيم
موضع تساؤل
ولكن ربما قمنا بحل هذه المشكلة
الأصابع عقدت
 
دراساتنا الإستقصائية الفضائية كشفت أن كوننا المنظور
مليء بمئات المجرات, وكل واحدة من هذه المجرات
يضم العديد من النجوم
النور الساطع لهذه النجوم المضيئة يمتص
بشكل واضح بواسطة الغبار والغاز داخل هذه المجرات
عندما نستنبط ملاحظاتنا لكامل الكون المرصود
نجد مليارات التريليونات من الشموس بالكثير من الكتلة
ورغم ذلك, عرفنا لبعض الوقت أن حوالي 95%
من محتوى طاقة الكون
هو في المادة المظلمة والطاقة المظلمة

English: 
[MUSIC PLAYING]
 For years,
astronomers have been
unable to find up to half of
the matter in the universe.
The missing baryon problem put
into question understanding
of the physics of the Big Bang.
We may just have solved it.
Fingers crossed.
[MUSIC PLAYING]
Our astronomical surveys have
revealed an observable universe
full of hundreds of billions
of galaxies, each of them
with as many stars.
The shining light of these stars
illuminates or is conspicuously
absorbed by gas and dust
within those galaxies.
When we extrapolate observations
to the entire observable
universe, we find a billion
trillion suns worth of mass.
However, we've known for
some time that around 95%
of the energy content
of the universe
is in dark matter
and dark energy.

French: 
Pendant des années, les astronomes étaient incapables
de détecter près de la moitié de la masse de l'univers
le mystère des baryons manquants
remettait en question notre compréhension de la physique du big bang
nous l'avons sans doute résolu … croisons les doigts !
Nos observations astronomiques ont révélé un univers
observable empli de centaines de milliards de galaxies
chacune composée de nombreuses étoiles
La lumière de ces étoiles illumine ou est
absorbée de façon évidente par
du gaz ou de la poussière dans ces galaxies
Quand nous extrapolons ces observations à l'ensemble
de l'univers observable
nous trouvons une masse de 
milliards de billions de Soleils
Cependant nous savons depuis un certain temps
qu'environ 95% du contenu en énergie de l'univers
est composé de matière noire et d'énergie noire

Portuguese: 
de encontrar cerca da metade de toda a matéria
O problema do  mistério do bárion
da física
Mas parece que
 
nosso entendimento
Nossas pesquisas astronômicas têm
revelado um um universo observável cheio de centenas de bihões
de galáxias , cada uma delas com muitos bilhões de estrelas
a luz brilhante dessas estrelas
é conspicuamente  absorvida pelo gás  e pó
dentro dessas galáxias. Quando
nós extrapolamos nossas observações para o inteiro
universo observável nós encontramos um bilhão de trilhão
de sóis dignos de massa. Contudo
nós sabemos por algum tempo que cerca de 95 por cento
da energia contida
no universo é matéria escura e energia escura.
Esse setor escuro
não interage com a luz
de nenhuma maneira e assim é invisível para nós.
O restante 5 por cento do setor iluminado representa
toda matéria regular do universo, sim
e se eu disser pra você que
todas as estrelas e galáxias e aglomerados de galáxias
somente corresponde a 10 por cento
do setor iluminado
o resto tem se mostrado tão invisível como o
escuro .
Nós pensamos que deve existir um extremamente difuso
gás entre as galáxias sim
mas nossas intensivas buscas falham
acima de meio passo.

English: 
For years, astronomers have been unable to
find up to half of the matter in the universe.
The missing Baryon problem put into question
our understanding of the physics of the Big Bang.
But we may just have solved it.
Fingers crossed.
Our astronomical surveys have revealed an
observable universe full of hundreds of billions of Galaxies.
Each of them with as many stars.
The shining light of these stars illuminates,
or is conspicuously absorbed by,
gas and dust within those galaxies.
When we extrapolate our observations to the entire observable universe,
we find a billion-trillion suns worth of mass.
However, we've known for sometime
that around 95% of the Energy-content of the Universe...
is in Dark Matter and Dark Energy.

English: 
This "Dark Sector" doesn't interact with Light in any way,
and so, is invisible to us.
The remaining 5%, the "Light Sector",
represents all of the regular matter in the universe.
Yet, what if I told you...
that all of the stars, and galaxies, and galaxy-clusters...
only comprise 10% of the light-sector.
The rest has proved as elusive as the dark-sector.
We think it must exist as really diffuse gas,
in-between the galaxies;
yet our intensest searches miss up to half of it.
At least until now.
First, a quick refresher on Dark-Matter and Dark-Energy:
and there's plenty more detail in som previous episodes.
Dark-Matter is believed to be an invisible...stuff...
that interacts only through gravity.
It comprises 80% of the Mass of the Universe,
or around 25% of its [The Universe] total energy-content.

English: 
This dark sector doesn't
interact with light in any way
and so is invisible to us.
The remaining 5%,
the light sector,
represents all of the regular
matter in the universe.
Yet, what if I told you
that all of the stars
and galaxies and galaxy
clusters only comprise
10% of the light sector?
The rest has proved as
elusive as the dark sector.
We think it must exist
as extremely diffuse gas
in between the galaxies.
Yet, our intense searches miss
up to half of it, at least
until now.
First, a quick refresher on
dark matter and dark energy.
And there's plenty more detail
in some previous episodes.
Dark matter is believed to
be an invisible stuff that
interacts only through gravity.
It comprises 80% of the mass
of the universe or around 25%
of its total energy content.

Arabic: 
هذا الجزء المظلم لا يتفاعل مع الضوء ولا بأي طريقة
وبالتالي هو غير مرئي بالنسبة لنا
ال 5% التي بقيت والتي تشمل الجزء المضيء
تمثل كل المادة النظاميّة في الكون
ولكن ماذا لو أخبرتك أن كل النجوم
والمجرات والعناقيد المجريّة
تضم فقط 10% من هذا الجزء المضيء
بقيّة الجزء تم إثبات أنه بعيد المنال كما الجزء المظلم
نحن نظن أنه يجب أن يوجد بشكل غاز منتشر بشكل كبير
بين المجرات
وحتى الأن بحثنا المكثّف يفتقد إلى نصفه, على الأقل
حتى الآن
في البداية مراجعة سريعة للمادة المظلمة والطاقة المظلمة
وهناك تفاصيل كثيرة ووفيرة في بعض حلقاتنا السابقة
المادة المظلمة يعتقد أنها مواد غير مرئية والتي
تتفاعل فقط عبر الجاذبية
وهي تضم 80 % من كتلة كوننا أوحوالي 25% من
المحتوى الطاقي الكامل للكون

Portuguese: 
até agora.
Primeiro um rápido resumo sobre energia escura e matéria escura
e aqui está um vídeo anterior com muitos mais detalhes .
Matéria escura é considerado ser uma substância invisível
que interage somente
com a gravidade e abrange
80 por cento da massa do universo ou cerca
25 por cento da energia contida nele.
Sua gravidade mantém as galáxias unidas e governam
o crescimento das estruturas de grande escala
através do tempo cósmico.
Assim onde matéria escura atrai
energia escura escura exerce sua antigravidade
e faz
a expansão do universo acelerar.
Essa energia do vácuo abrange
70 por cento da
energia contida no universo
o restante 5 por cento é matéria
bariônica regular.
A maneira que  nós chamamos um bárion é um próton ou um nêutrom de 3/4
mas realmente matéria bariônica se refere
a matéria das estrelas planetas gás

French: 
Ce «secteur noir» n'interagit en aucune façon
avec la lumière, et nous est donc invisible.
Les 5% restant, le «secteur de la lumière»,
représente toute la matière normale de l'univers.
Et si je vous disais que
toutes les étoiles, galaxies et amas de galaxies
ne représentent que 10% du «secteur de la lumière».
le reste est aussi difficile à trouver
que le «secteur sombre»
Nous pensons qu'il doit exister
sous la forme d'un gaz très diffus
entre les galaxies.
Et pourtant nos recherches intenses n'en trouvent pas
près de la moitié
Enfin, jusqu'à présent.
Mais d'abord un petit rappel sur la 
matière noire et l'énergie noire
Vous trouverez plein de détails
dans un épisode précédent.
La matière noire est supposée être un «truc» invisible
qui n’interagit que gravitationnellement.
Elle compose 80% de la masse de l'univers
soit à peu près 25% de son contenu en énergie.

English: 
Its [Dark-Matter] gravity holds galaxies together,
and governed the growth of large-scale structure
in our universe throughout cosmic time.
Now where Dark-Matter pulls,
Dark-Energy pushes.
It's anti-gravitational...
and causes the expansion of the universe to accelerate.
This... energy of the vacuum
comprises 70% of the Universe's energy-content.
The remaining 5% is regular Baryonic matter.
By the way, a Baryon,
is a three-quark particle like a proton or a neutron;
but really, baryonic matter refers to
Atomic matter. It's the stuff of stars, planets,
gas, dust, you me.
Baryonic matter interacts with light,
so we can search for it by scanning the electromagnetic spectrum.
Except, by doing so, we miss most of it.
This is the 'missing baryon problem'.
There's a huge discrepancy between the amount of

Arabic: 
جاذبيتها تمسك المجرات معاً
وتحكم نمو البنى على النطاق الواسع
في كوننا على مدار مقياس الوقت الكوني
الآن عندما المادة المظلمة تسحب الطاقة المظلمة تدفع
إنها مضادة للجاذبية وتسبب
تسارع في توسع الكون
طاقة الفراغ هذه تضم 70 % من محتوى طاقة الكون
 
ال 5% الباقية هي مادة باريونيّة
وبالمناسبة الباريون يتألف من 3 جسيمات كوارك
كالبروتون والنيوترون
ولكن في الحقيقة المادة الباريونيّة تشير إلى المادة الذريّة
إنها المواد التي تتألف منها النجوم والكواكب والغاز, الغبار, أنت , أنا ...
المادة الباريونيّة تتفاعل مع الضوء
وبالتالي يمكننا البحث عنها عن طريق مسح
الطيف الكهرومغناطيسي
بإستثناء أنه بفعلنا هذا نفقد معظمها
وهذه هي مشكلة المادة الباريونيّة المفقودة
هناك تناقض كبير بين مقدار

Portuguese: 
você e eu.
Matéria bariônica interage com a luz assim nós
podemos escanear o espéctro elétro magnético
por
fazer assim nós perdemos a maioria
dele.
Esse é o problema da variante perdida.
Há uma grande discrepância entre a quantidade de matéria bariônica
encontrada em nossas buscas e
as teorias. Deve haver algo lá fora e estas
teorias são muito sólidas.
Por exemplo, nos primeiro minutos após o big bang o hidrogênio
se fundiu em deutério e hélio
o repositório de hidrogênio que
que terminou sendo convertido é muito dependente
da densidade desse hidrogênio assim a
massa bariônica.
Por medir a quantidade relativa de hélio e deutério hoje sabemos
deve ter havido dez vezes mais hidrogênio
pra começar do que o que nós vemos hoje em dia
em galáxias e aglomerados
e a segunda maneira  de calcular a massa bariônica  esperada é

French: 
Ses effets gravitationnels donnent 
leur forme aux galaxies
et détermine la croissance des grandes
structures de notre univers tout au long de son histoire
Maintenant, là où la matière est attractive
l'énergie noire est répulsive.
Elle est anti gravitationnelle et
provoque l'accélération de l'expansion de l'univers.
Cette énergie du vide
représente 70% du contenu énergétique de l'univers.
Les 5% restants sont composés de
matière baryonique normale.
À propos, un baryon est une particule composée de 3 quarks comme un proton ou un neutron.
Mais la matière baryonique est en fait la matière composée d'atomes.
C'est ce qui compose les étoiles, les planètes, le gaz, la poussière, vous, moi.
La matière baryonique interagit avec la lumière,
nous pouvons donc la rechercher en scrutant
le spectre électromagnétique.
Sauf qu'en cherchant de la sorte, 
la plus grande part nous échappe
C'est le mystère des baryons manquants.

English: 
Its gravity holds
galaxies together
and governed to the growth
of large-scale structure
in our universe
throughout cosmic time.
Now where dark matter
pools, dark energy pushes.
It's anti-gravitational
and causes the expansion
of the universe to accelerate.
This energy of the vacuum
comprises 70% of the universe's
energy content.
The remaining 5% is
regular baryonic matter.
By the way, a baryon
is a 3-quark particle
like a proton or a neutron.
But really, baryonic matter
refers to atomic matter.
It's the stuff of stars,
planets, gas, dust, you, me.
Baryonic matter
interacts with light,
so we can search
for it by scanning
the electromagnetic spectrum.
Except, by doing so,
we miss most of it.
This is the missing
baryon problem.
There's a huge discrepancy
between the amount

English: 
of baryonic matter
our surveys find
and the amount that our theories
say should be out there.
And those theories
are pretty solid.
For example, in the
first several minutes
after the Big Bang,
hydrogen fused
into deuterium and helium.
The proportion of hydrogen
that ended up getting fused
is very dependent on the
density of that hydrogen, so
the baryonic mass.
Measuring the relative abundance
of helium and deuterium today
tells us that there should have
been 10 times as much hydrogen
to start with than
we actually see today
in galaxies and clusters.
The second way to calculate
the expected baryonic mass
is with the cosmic microwave
background radiation.
Perhaps, you
remember this stuff.
It's the light
released at the moment
the first atoms formed nearly
400,000 years after the Big
Bang.
We still see that light
today traveling to us
from distant parts.
It carries with it a map of
the structure of the cosmos

Arabic: 
المادة الباريونية التي وجدناها بدراستنا الإستقصائية
وبين المقدار الذي تنبأت به نظرياتنا
وهذه النظريات متينة ووثيقة
على سبيل المثال, في الدقائق العديدة الاولى
بعد الإنفجار الكبير, الهيدروجين إنصهر
إلى الديتريوم والهيليوم
نسبة الهيدروجين المنصهرة
تعتمد بشكل كبير على كثافة هذا الهيدروجين
وبالتالي على كتلة المادة الباريونيّة
قياس الوفرة النسبيّة من الهيليوم والديتريوم اليوم
يخبرنا أن كمية الهيدروجين يجب أن تكون أكثر بعشر مرات من كميّة الهيدروجين
التي تشكلت في بداية الكون وهذا كما نراه الآن
في المجرات والعناقيد المجرية
الطريقة الثانية لنحسب المادة الباريونيّة المتوقعة
هي بإستخدام إشعاع الخلفيّة الميكروية الكوني
ربما تذكر هذه الأمور
إنه الضوء المتحرر في اللّحظة
التي تشكلت بها الذرات أي حوالي 400,000 سنة بعد الإنفجار الكبير
 
لا نزال نرى هذا الضوء إلى اليوم وهو يسافر إلينا
من الأجزاء البعيدة
وهو يحمل معه خريطة لبنية الكون

Portuguese: 
a radiação de microondas de fundo
provavelmente você se lembra que essa coisa é a luz  liberada
no momento da formação dos primeiros átomos 400.000 anos após o big bang;
até
nós de distantes partes.
Ela traz com ela um mapa da estrutura do universo daqueles primeiros tempos.
Essas bolhas são flutuações
na densidade que iria mais tarde
colapsar para se tornar aglormerados de galáxias e
por analizar essas flutuações nós podemos
calcular a quantidade relativa de  barions
para a matéria escura.
Veja que os fótons da radiação cósmica de fundo
liberados foram aprisionados
no fluxo de plasma quente da
matéria bariônica . A inter relação entre bárions e
e fótons resultou em oscilações na densidade
ondulando as regiões externas de alta densidade
essas ondulações bariônicas acústicas ajudaram
a produzir uma pequena família de bolhas
comparadas às grandes bolhas no mapa da CMB
Essas grandes bolhas são conduzidas pela matéria escura que

English: 
Baryonic matter our surveys find,
and the amount our theories say should be out there.
And those theories are pretty solid. For example:
in the first few seconds after the Big-Bang,
Hydrogen fused into Deuterium and Helium.
The proportion of Hydrogen that ended up getting fused
is fairly dependent on the density of that Hydrogen.
So, the Baryonic Mass.
Measuring the relative abundance of Hydrogen and Deuterium today
tells us there should have been ten-times as much Hydrogen to start with,
than we actually see today in galaxies and clusters.
The second way to calculate the expected baryonic-mass
is with the cosmic microwave background radiation.
Perhaps you remember this stuff,
it's the light released the moment the first atoms formed
nearly 400 000 years after the Big-Bang.
We still see that light today
travelling to us from distant paths.
It carries with it a map of the structure of the cosmos from those early times.

French: 
Il y a une grande différence entre la quantité
de matière baryonique
mise en évidence par nos recherches
et les quantités prédites par nos théories.
Et ces théories sont assez solides,
par exemple, dans les premières minutes
après le big bang
l'hydrogène a fusionné pour donner naissance
à du deutérium et de l'hélium.
La proportion d'hydrogène fusionné dépend fortement de la densité de cet hydrogène ;
et donc de la masse de matière baryonique.
La mesure de l'abondance relative actuelle d'hélium et de deutérium
nous indique qu'il y devait y avoir
10 fois plus d'hydrogène au départ
que ce que nous voyons aujourd'hui
dans les galaxies et les amas.
La deuxième méthode pour prédire la masse baryonique
utilise le fond diffus cosmologique.
Peut vous souvenez-vous de ça,
Il s'agit de la lumière émise lors de la
formation des premiers atomes
environ 400.000 ans après le big bang.
Nous pouvons toujours observer cette lumière, voyageant vers nous de régions éloignées.
Elle crée une carte de la structure
du cosmos à cette époque.

French: 
Ces petites taches sont des fluctuations dans la densité
qui plus tard s'effondreront plus tard
en amas de galaxies.
Et en analysant ces fluctuations,
nous pouvons déterminer l'abondance relative des baryons par rapport à la matière noire
Voyez-vous, avant que les photons du fond diffus cosmologique n'aient été émis,
ils étaient piégés dans le plasma extrêmement
chaud de la matière baryonique
Les interactions entre les baryons et le photon ont donné naissance à des oscillations de densité,
un peu comme des ondes sonores sortant d'une région de forte densité.
Ces «oscillations acoustiques baryoniques»
ont contribuées à créer un groupe de petites taches
plus petit comparé aux plus grandes taches de la carte du fond diffus cosmologique.
La forme de ces grandes taches sont
déterminées par la matière noire,
qui n'interagit pas avec la lumière
et ne peut donc créer des oscillations de densité.
En analysant la distribution des tailles des taches
dans ce que nous appelons le spectre de puissance
du fond diffus cosmologique,

English: 
These speckles are fluctuations in density
that would later collapse to become the galaxy-clusters.
And by analyzing these fluctuations,
we can figure out the relative abundance of baryons to Dark-Matter.
See, before the photons of the cosmic microwave background were released
they were trapped in the searing hot plasma of baryonic matter.
The interplay between baryons and photons
resulted in density oscillations.
Much like sound waves rippling outwards from high-density regions,
these baryonic acoustic oscillations
helped produce a smaller family of speckles,
compared to the largest blobs on the CMB map.
Those large blobs are driven by dark-matter
which doesn't interact with light
so it can't produce density oscillations.
By analyzing the distribution in speckle sizes
with what we call the "CMB" Power-Spectrum,

Arabic: 
من هذه الأوقات الباكرة
هذه البقع هي تقلبات في الكثافة
والتي ستنهار في وقت لاحق لتشكل العناقيد المجرية
وبتحليل هذه التقلبات
يمكننا معرفة الوفرة النسبيّة للمادة الباريونيّة
إلى المادة المظلمة
لاحظ, قبل أن تتحرر فوتونات إشعاع الخلفيّة الميكرويّة
كانت هذه الفوتونات حبيسة البلازما الحارقة والشديدة السخونة
للمادة الباريونية
التفاعل بين المادة الباريونيّة والفوتونات
أدى إلى تذبذبات في الكثافة
كموجة الصوت الممتدة إلى الخارج
من منطقة عالية الكثافة, هذه التذبذبات الصوتية الباريونية
ساعدت في إنتاج عائلة صغيرة من البقع
مقارنة بالنقط الكبيرة في خريطة إشعاع الخلفيّة الميكرويّة
هذه النقط الكبيرة مقادة بالمادة المظلمة والتي
لا تتفاعل مع الضوء, وبالتالي لا يمكنها
إنتاج تذبذبات كثافة
بتحليل توزّع وحجوم البقع
في ما نسمية الطيف القوي لإشعاع الخلفيّة الميكرويّة

English: 
from those early times.
These speckles are
fluctuations in density
that would later collapse to
become the galaxy clusters.
And by analyzing
these fluctuations,
we can figure out the
relative abundance of baryons
to dark matter.
See, before the photons of the
cosmic background radiation
were released, they were trapped
in the searing hot plasma
of baryonic matter.
The interplay between
baryonic and photons
resulted in density
oscillations.
Much like sound waves
rippling outwards
from high density regions, these
baryonic acoustic oscillations
helped produce a smaller
family of speckles
compared to the largest
blobs on the CMB map.
Those large blobs are
driven by dark matter, which
doesn't interact with
light, so it can't
produce density oscillations.
By analyzing the distribution
and speckle sizes
in what we call the
CMB power spectrum,

Portuguese: 
não interage com  a luz assim ela não pode
produzir  oscilações de densidade para ser analizadas.
A distribuição no tamanho das bolhas
que nós chamamos energia do espectro da CMBi
Nós encontramos a quantidade relativa de bárions comparados
com a matéria escura.
De novo nós calculamos que deve existir muito mais matéria bariônica do que
nós vemos nas galáxias,
seguindo a contínua liberação de radiação de cósmica de fundo.
A gravidade continuou a fazer o seu trabalho e colapsou nessas fracas flutuações
em gigantescos aglomerados de galáxias.
Simulações em supercomputadores revelaram
a forma dessa estrutura de grande escala
resultantes do colapso gravitacional.
E é como rios  na teia cósmica
e faixas de matéria escura fluindo
em gigantes redemoinhos arrastando
matéria bariônica com eles e
as ligações entre filamentos de matéria
é densa  o suficiente para as galáxias  serem formadas .

Portuguese: 
Nossas pesquisas de galáxias confirmam que
é com isso que essas estruturas de escalas gigantescas no univeverso se parecem
e ainda quando
nós somamos a massa dessas galáxias
a maior parte da matéria bariônica predita por nossas teorias
está faltando e assim onde ela está
A gravidade continuou a fazer o seu trabalho e colapsou nessas fracas flutuações
em gigantescos aglomerados de galáxias.
Simulações em supercomputadores revelaram
a forma dessa estrutura de grande escala
resultantes do colapso gravitacional.
E é como rios  na teia cósmica
e faixas de matéria escura fluindo
em gigantes redemoinhos arrastando
matéria bariônica com eles e
as ligações entre filamentos de matéria
é densa  o suficiente para as galáxias  serem formadas .
Nossas pesquisas de galáxias confirmam que
é com isso que essas estruturas de escalas gigantescas no univeverso se parecem
e ainda quando
nós somamos a massa dessas galáxias
a maior parte da matéria bariônica predita por nossas teorias

French: 
nous pouvons déterminer la quantité de matière baryonique
en fonction de la quantité de matière noire.
À nouveau, nous prédisons qu'il devrait y avoir beaucoup plus de matière baryonique
que ce que nous observons dans les galaxies.
Faisant suite à l'émission du fond diffus cosmologique,
la gravité continue d'agir
et fait s'effondrer ces faibles fluctuations
dans des amas de galaxies gargantuesques.
Des simulation menées sur des super ordinateurs
révèlent la forme de ces structures à grandes échelles
qui devraient être issues de cet
effondrement gravitationnel.
C'est la toile cosmique.
Des rivières et des feuilles de matière noire
coulent en des halos géants de matière noire
entraînant la matière baryonique avec elles.
Dans les nœuds entre les filaments,
la matière est suffisamment dense
pour former des galaxies.
Nos observations des galaxies confirment que c'est à quoi ressemblent les grandes structures de l'univers
Et pourtant, quand nous additionnons 
la masse de ces galaxies,
la plupart de la matière baryonique prédite par
nos théories est manquante.
Alors, où est-elle ?

Arabic: 
يمكننا إيجاد الكميّة النسبيّة من المادة الباريونيّة مقابل المادة المظلمة
وللمرة الثانية, حساباتنا أظهرت أنه يجب أن يكون هناك مادة باريونية
أكثر مما نراه في المجرات
بإتباع إشعاعات الخلفيّة الميكرويّة الكونية المتحررة
الجاذبيّة تستمر بعملها مسببة إنهيار هذه
التذبذبات الباهتة إللى عناقيد مجريّة عملاقة
 
تظهر محاكاة الكمبيوترات الخارقة شكل هذه البنى الضخمة
على النطاقات الواسعة
والتي يجب أن تنتج من الإنهيار الجذبوي
إنها الشبكة الكونية
أنهار وأوراق من المادة المظلمة تتدفق إلى هالات عملاقة
من المادة المظلمة
ساحبة المادة الباريونيّة معها
في الروابط بين الخيوط, المادة
كثيفة بشكل كافي لتشكل المجرات
الآن دراساتنا الإستقصائية للمجرات تؤكد
أن هذا ما تبدو عليه البنى على النطاق الواسع لكوننا
 
وبرغم هذا, عندما نضيف الكتلة من هذه المجرات
معظم المادة الباريونيّة المتنبأ بها بواسطة النظرية تكون مفقودة
 
إذاً أين هي..؟

English: 
we can find the relative amount
of baryonic versus dark matter.
Again, we calculate that they
should be way more baryonic
matter than we see in galaxies.
Following the release of the
cosmic background radiation,
gravity continued to do
its work and collapse
these faint fluctuations
into gargantuan clusters
of galaxies.
Supercomputer simulations
reveal the shape
of this large-scale
structure that
should result from this
gravitational collapse.
It's the cosmic web.
Rivers and sheets of dark matter
flow into giant dark matter
halos, dragging baryonic
matter with them.
In the nexuses between
filaments matter
is dense enough for
galaxies to form.
Now surveys of galaxies
confirm that this
is what the large-scale
structure of the universe
looks like.
And yet, when we add up the
mass from those galaxies,
most of the baryonic matter
predicted by a theory
is missing.
So where is it?

English: 
we can find the relative amount of baryonic vs. dark-matter.
Again, we calculate that there should be way more baryonic matter
than we see in galaxies.
Following the release of the cosmic microwave background radiation,
Gravity continued to do its work,
and collapse these faint fluctuations
into gargantuan clusters of galaxies.
Super-computer simulations reveal
the shape of this large-scale structure
that should result from this gravitational collapse.
It's the Cosmic Web.
Rivers and sheets of Dark-matter
flow into giant dark-matter Halos,
dragging baryonic matter with them.
In the Nexuses between filaments,
matter is dense enough for galaxies to form.
Our surveys of galaxies confirm this is what the large-scale structure of the universe looks like.
And yet, when we add up the mass from those galaxies
most of the baryonic matter predicted by our theory...
is missing... So where is it?

Portuguese: 
está faltando e assim onde ela está
Nossa melhor suposição é que ela está na forma de
muito difuso plasma na forma de
átomos que foram despojados de seus elétrons e se encontram entre as galáxias
Agora alguma da matéria nós poderíamos ver se
se o plasma estiver quente o suficiente então vai emitir
raios x que podem ser detectados.
Nós tipicamente vemos essa matéria dentro de aglomerados de galáxias onde
o plasma é relativamente denso e
energizado pela luz da próprias galáxias .
Por outro lado
se a substância é fria o suficiente então o núcleo pode
recapturar os elétrons e se tornar um gás em vez de um plasma.
Esse gás absorve
a assinatura dos comprimentos das ondas de luz que
passa através dele.
Essa característica de absorção na luz de distantes quasars
revela esse fino gás à espreita
entre aglomerados de galáxias.
Contudo por olhar somente no material aquecido ou no resfriado
nós não encontramos nem de longe  a

English: 
Well, our best guess is that it's in the form of a very diffuse form of plasma.
Atoms, stripped of their electrons, in between the galaxies.
Now, some of that stuff we can see:
if the plasma is hot enough it emits detectable X-Rays.
We typically see that stuff inside galaxy-clusters,
where the plasma is relatively dense,
and is energized by the light of the galaxies themselves.
On the other hand,
if the material is cool enough, then nuclei can recapture their electrons,
and become a gas instead of a plasma.
This cool gas then absorbs signature wavelengths from light that passes through it.
Absorption features in the light of distant Quasars
reveal this gas lurking between the clusters of galaxies.
However, by looking only at the hottest or coolest material,
we don't find nearly enough of it
to account for missing Baryons.

French: 
Bon, notre meilleure hypothèse
est qu'elle soit sous la forme d'un plasma très diffus,
des atomes séparés de leurs électrons,
entre les galaxies.
Bon, nous pouvons en observer une partie.
Si le plasma est suffisamment chaud, 
alors il émet des rayons X détectables.
Nous l'observons habituellement
dans les amas de galaxies
où le plasma est relativement dense
et est excité par la lumière même de ces galaxies.
D'un autre côté, si le matériau est suffisamment froid,
alors les noyaux peuvent recapturer des électrons
pour former un gaz au lieu de plasma.
Ce gaz froid absorbe alors des longueurs d'ondes particulières de la lumière qui le traverse.
Ces absorptions caractéristiques dans
la lumière de quasars lointains
révèlent ce gaz se tapissant entre les amas de galaxies.
Malgré tout, en ne regardant que les matériaux
les plus froids ou les plus chauds
nous n'en trouvons pas assez pour expliquer
le mystère des baryons manquants.

English: 
Well, our best
guess is that it's
in the form of a very
diffuse plasma, atoms
stripped of their electrons
in between the galaxies.
Now some of that
stuff we can see.
If the plasma is
hot enough, then it
emits detectable X-rays.
We typically see that stuff
inside galaxy clusters
where the plasma
is relatively dense
and is energized by the light
of the galaxies themselves.
On the other hand, if the
material is cool enough,
then nuclei can
recapture their electrons
and become a gas
instead of a plasma.
This cool gas then absorbs
signature wavelengths
from light that
passes through it.
Absorption features in the
light of distant quasars
reveal this gas lurking
between clusters of galaxies.
However, by looking
only at the hottest
or the coolest material, we
don't find nearly enough of it
to account for the
missing baryons.
It seems that the
missing material

Arabic: 
حسناً, أفضل تخميناتنا هي أنها
في شكل بلازما منتشرة بشكل كبير
الذّرات جرّدت من إلكتروناتها بين المجرات
الآن بعض من هذه الأمور يمكننا رؤيتة
إذا كانت البلازما حارة بشكل كافي, عندها
سوف تشع إشعاعات إكس التي يمكن كشفها
نحن نرى عادة هذه الأشياء داخل العناقيد المجرية
حيث البلازما تكون كثيفة بشكل نسبي
ومنشّطة بواسطة ضوء المجرات نفسها
ومن ناحية أخرى, إذا كانت المواد باردة بشكل كافي
عندها يمكن للنوى أن تسترد إلكتروناتها
متحولة إلى غاز بدلاً من البلازما
هذه الغاز البارد يمتص الطول الموجي الخاص به(والذي يعبر عنه)
من الضوء الذي يعبر خلاله
خصائص إمتصاص الضوء للكوازارات البعيدة
تكشف أن هذا الغاز يتموضع بين عناقيد المجرّات
ومع ذلك, بالنظر إلى المواد الأسخن
أو الأبرد فقط, نحن لا نجد بما فيه الكفاية منها
لحساب المادة الباريونيّة المفقودة
ما يبدو هو أن هذه المواد المفقودة

Portuguese: 
quantidade para dar conta do bárion faltante.
Parece que o material que falta deve estar
na faixa de temperatura intermediária
assim ele deve ser quente o suficiente para ainda ser plasma
caso contrário  iria produzir características de absorção mas
mas ele  não pode ser assim tão quente ou denso para emitir raios x
que podemos detectar ,assim isso nos diz que o melhor
lugar para procurar o barion perdido
É nos gigantes filamentos que formam
a teia cósmica  se estendendo entre os aglomerados de galáxias.
Esse material deve ser mais frio
que os aglomerados mas deve
ser quente o suficiente para pelo menos formar o plasma
visto. Os vastos efeitos de maré em galáxias próximas
cria colisões que aquece esses bárions
a centenas de milhares ou mesmo milhões de kelvin
ao mesmo tempo
essa matéria  esperada ser extremamente
de baixa densidade somente cerca de dez vezes
a do espaço intergalático o que faz dela o mais perfeito
vácuo que qualquer outra coisa que nós podemos criar em laboratório
ou mesmo que existe na via láctea.

English: 
must be in the intermediate
temperature range.
It must be hot enough
to still be a plasma.
Otherwise, it would produce
absorption features.
But it can't be so hot or dense
as to emit detectable X-rays.
This tells us that the best
hiding place for the missing
baryons is the
giant filaments that
form the cosmic web stretching
in between galaxy clusters.
That material would be cooler
than the clusters themselves,
but should at least be hot
enough to form a plasma.
See, the vast tidal
effects of nearby galaxies
create shocks that
can heat those baryons
to hundreds of thousands
or even millions of Kelvin.
At the same time,
this stuff is expected
to be extremely low-density,
only around 10 times
that of intergalactic space.
That makes it a more
perfect vacuum than anything
we've created in a lab or
even exists in the Milky Way.

French: 
Il semble que la température du
 matériau manquant se situe
dans l'intervalle intermédiaire :
suffisamment chaud pour demeurer un plasma
sinon il produirait des raies d'absorption ;
sans l'être de trop pour émettre
 des rayons X détectables.
Cela nous indique que le meilleur endroit pour les baryons manquants
sont les filaments géant formant la toile cosmique
s'étendant entre les amas de galaxies.
Ce matériau serait plus froid que les amas
tout en restant suffisamment 
 chaud pour former un plasma.
Voyez-vous, les immenses effets de marée
dans le voisinage des galaxies
créent des chocs qui peuvent chauffer ces baryons
à des centaines de milliers
ou même des millions de kelvins.
En même temps, on s'attend à le trouver à des densités très basses.
Seulement 10 fois la densité de l'espace intergalactique.
Ce qui en fait un vide supérieur à ce que
nous pouvons créer en  laboratoire,
ou même que l'on trouve dans la Voie-Lactée.
Et pourtant, ces flaments sont immenses ;

Arabic: 
عليها أن تكون في نطاق درجة الحرارة المتوسطة
أي يجب أن تكون حارة بشكل كافي لتظل في حالة البلازما
وإلا ستنتج خاصيات إمتصاصيّة
ولكن لا يمكنها أن تكون حارة أو كثيفة كثيراً لتشع أشعة إكس يمكن رصدها
وهذا يخبرنا أن أفضل مكان لإختباء هذه الباريونات
هي في الخيوط العملاقة التي
تشكل الشبكة الكونية والتي تمتد بين العناقيد المجريّة
تلك المواد ستكون أبرد من العناقيد بذاتها
ولكن يجب على الأقل أن تكون حارة بشكل كافي لتشكل البلازما
لاحظ أن تأثر السحب والدفع من المجرات القريبة
يخلق صدمات يمكنها أن تسخن هذه الباريونات
إلى مئات آلاف وحتى ملايين الكلفنات
وفي نفس الوقت هذه المواد يتوقع
أن تكون بكثافة منخفضة جداً, فقط حوالي 10 مرات
من الكثافة الموجودة بين فضاء المجرات نفسها
وهذا يخلق فضاء أكثر مثالية من أي شيء
صنعناه في المختبرات, أو في أي فضاء موجود في درب التبانة

English: 
It seems that the missing material must be in the 'intermediate' temperature range;
it must be hot enough to still be a plasma,
otherwise it would produce absorption features.
But it can't be so hot or dense as to emit detectable X-Rays.
This tells us that the best hiding place for the missing Baryons
is the giant filaments that form the cosmic web,
stretching in-between galaxy-clusters;
that material would be cooler than the clusters themselves,
but should, at least, be hot enough to form a plasma.
See, the vast tidal effects of nearby galaxies
create shocks that can heat those Baryons to hundreds of thousands, or even millions of Kelvin.
At the same time, this stuff is expected to be extremely low density,
only around ten-times that of intergalactic space.
That makes it a more perfect vacuum than anything we've created in a lab,
or even exists in the Milky Way.
And yet, those filaments are vast,

English: 
tens of millions of Lightyears long;
and so, those solitary Baryons could add up
to more mass than all of the galaxies in the universe.
So, how do we spot this stuff?
Two research groups have figured it out.
The secret is: the "Thermal Sunyaev-Zel'Dovich Effect".
We talked about the Kinetic S-Z Effect in our episode on Dark-Flow.
The Thermal SZ is similar.
And again, it makes use of the cosmic microwave background.
As photons from the CMB pass through a giant filament,
the hot plasma in the filament grants it a little energy-boost.
In fact, the electrons in that plasma scatter CMB photons to higher energies.
So, if there's enough of this stuff,
then the CMB map should be slightly hotter
directly in-between galaxies that are connected between filaments.

French: 
des dizaines de millions d'années-lumière de long.
Ainsi la somme des masses de ces baryons solitaires
pourrait être plus grande que la masse de la totalité
des galaxies de l'univers.
Alors, comment repérons-nous ce truc ?
Deux groupes de recherche ont résolu le problème.
Le secret est l'effet Sunyaev-Zel'dovich thermique.
Nous avons abordé l'effet Effet Sunyaev-Zel'dovich cinétique
dans l'épisode «Dark Flow».
L'effet SZ Thermique est similaire
et utilise à nouveau le fond diffus cosmologique.
Un photon du fond diffus cosmologique
qui traverse un filament géant
gagne un peu d'énergie du plasma chaud.
En fait, les électrons dans ce plasma
dispersent ces photons vers des énergies plus grandes.
Donc s'il y assez de cette matière,
la carte du fond diffus devrair apparaître
légèrement plus chaude
entre les galaxies connectées par un filament.
Et, il s'avère qu'e c'est plus chaud.

English: 
And yet, those filaments
are vast, tens of millions
of light years long.
And so those solitary
baryons could add up
to more mass than all of the
galaxies in the universe.
So how do we spot this stuff?
Two research groups
have figured it out.
The secret is the thermal
Sunyaev-Zel'Dovich effect.
We talked about the kinetic
SZ effect in our episode
on dark flow.
The thermal SZ is similar.
And again, it makes use of the
cosmic microwave background.
As photons from the CMB pass
through a giant filament,
the hot plasma in the filament
grants it a little energy
boost.
In fact, the electrons
in that plasma scatter
CMB photons to higher energies.
So if there's enough
of this stuff,
then the CMB map should
be slightly hotter
directly in between
galaxies that
are connected by filaments.

Arabic: 
وحتى الآن, هذه الخيوط شاسعة بطول عشرات ملايين
السنين الضوئية
وبالتالي هذه الباريونات المعزولة يمكنها أن تضاف
إلى المزيد من الكتلة من كل المجرات في كوننا
إذاً, كيف نكتشف هذه الأشياء
فريقين من الباحثين إكتشفوا هذا
السر هو في تأثير زنايف زيلدوفيتش الحراري
تحدثنا عن تأثير زنايف زيلدوفيتش الحركي في حلقتنا عن التدفق المظلم (وهي مترجمة أيضاً إلى العربية)
 
تأثير زنايف زيلدوفيتش الحراري مشابه له
وللمرّة الثانية, إنه يجعلنا نستخدم شعاع الخلفيّة الميكرويّة الكوني
عندما تعبر الفوتونات من  شعاع الخلفيّة الميكرويّة عبر الخيوط العملاقة
البلازما الساخنة في الخيوط تمنحهم  دفعة طاقية صغيرة
 
في الحقيقة, الإلكترونات في تلك البلازما تبعثر
فوتونات شعاع الخلفية الكوني إلى طاقة أعلى
وبالتالي إذا كان هناك ما يكفي من هذه المواد
عندها خريطه  شعاع الخلفيّة الميكرويّة يجب أن تكون أسخن قليلاً
وبشكل مباشر بين المجرات
المتصلة بواسطة الخيوط

Portuguese: 
E ainda, esses filamentos são imensos
dezenas de milhões de anos luz de extensão e
assim esses barions solitários podem
possuir mais massa que todas as galáxias no universo.
Então como
nós podemos detetctar essa substância .
Dois grupos de pesquisa concluiram que
o segredo é o efeito thermal tsarnaev
zeldo vich .
Nós falamos sobre o efeito cinético SZ em nosso
episódio sobre o fluxo escuro . 
 O thermal SC
é parecido e de novo
ele faz uso da  radiação de micro onda de fundo
então os fótons da CMb
passam através de um filamento gigante
do plasma aquecido
e ganham um pequeno aumento de energia
e esse plasma espalha
os fótons para altas energias assim
se houver suficiente dessa substância  o mapa da  CMB
deve ser ligeiramente mais quente diretamente
entre galáxias que
estão conectadas por
por filamentos e acontece que

English: 
And... it turns out it is hotter.
Two teams, Graaf & collaborators, and Tanimura & collaborators,
just published the results of their attempts to look for the Sunyaev-Zel'Dovich Effect.
They both used the latest Planck-Satellite CMB map
in the presumed location of large-scale structure filaments,
which they assumed was between pairs of nearby massive galaxies.
The type typically found in:
Giant Dark-Matter Halos.
Now it wasn't an easy experiment.
The SZ effect is tiny,
and so the researchers needed to add together the results from many, many galaxy pairs.
Graaf et. al. used a-million galaxy pairs,
while Tanimura et. al. used about 260 000.
Both teams report detection of the Termal Sunyaev-Zel'Dovich effect
with around 5-Sigma significance; or to translate:
They found the Baryons.
These filaments seem to have enough of this hot, diffuse plasma

Arabic: 
وتبين أنها كذلك (أسخن)
فريقين, غراف ومجموعته وتانيمورا ومجموعته
نشروا نتائج
محاولاتهم في البحث عن تأثير زنايف زيلدوفيتش
كلاهما إستخدم خريطة شعاع الخلفيّة الميكرويّة الأخيرة من القمر الصناعي بلانك
من موقعهم المفترض لبنى الخيوط الكبيرة النطاق
والتي فرضوا أنها
بين أزواج المجرات القريبة الضخمة, النموذج عادةً
وحد في هلات المادة المظلمة العملاقة
في الحقيقة لم تكن تجربة سهلة
تأثير زنايف زيلدوفيتش كان صغير
وبالتالي الباحثين إحتاجوا أن يضيفوا نتائج
أزواج الكثير والكثير من المجرات معاً
غراف ومجموعته
إستخدموا مليون زوج مجري ببينما تانيمورا ومجموعته
إستخدموا 260,000 زوج مجري
كلا الفريقين كشفوا نتائجهم عن تأثير زنايف زيلدوفيتش الحراري
بحوالي 5 دلالات لسيغما
أو بترجمة أخرى, لقد وجدوا الباريونات
هذه الخيوط تبدو وكأنها تحوي كفاية من البلازما المنتشرة الساخنة

English: 
And it turns out it is hotter.
Two teams, Graaff and
collaborators and Tanimura
and collaborators, just
published the results
of their attempts to look for
the Sunyaev-Zel'Dovich Effect.
They both used the latest
Planck satellite CMB
map in the presumed locations
of large-scale structure
filaments, which
they assumed was
between pairs of nearby massive
galaxies, the type typically
found in giant
dark matter halos.
Now it wasn't an
easy experiment.
The SZ effect is tiny.
And so the researchers needed
to add together the results
from many, many galaxy pairs.
Graaff et al.
used a million galaxy
pairs, while Tanimura et al.
used 260,000.
Both teams report
detection of the thermal
Sunyaev-Zel'Dovich effect with
around 5 sigma significance.
Or to translate, they
found the baryons.
These filaments seem to have
enough of this hot diffuse

French: 
Deux équipes :
De Graaff et al. ainsi que Tanimura et al.
viennent de publier les résultats de leurs tentatives
pour mettre en évidence l'effet  Sunyaev-Zel'dovich
Tous deux ont utilisé la dernière carte 
du fond diffus du satellite Planck
aux localisations présumées de filaments reliant de grandes structures
qu'ils supposaient étaient entre des paires de galaxies massives
le genre habituellement observé dans les halos géants de matière noire.
Ce n'était pas une expérience facile.
L'effet SZ est faible.
Du coup les recherches devaient inclure les données de nombreuses paires de galaxies.
De Graaff et al. ont utilisé un million de paires
alors que Tanimura et al. en ont utilisé 260.000 .
Les deux équipes disent détecter l'effet SZ thermique
avec une confiance de 5 sigmas.
Ou, traduction,
ils ont trouvé les baryons.
Ces filaments semblent contenir suffisamment
de ce plasma chaud et diffus

Portuguese: 
ele é quente
Dois times graph collaborators e Tamara
collaborators acabam de publicar os resultados das suas tentativas de
observar o efeito tsarnaev zors ovitch
O dois usaram o mais novo mapa feito pelo satélite Planck
nos locais que se imagina
existir filamentos nas estruturas de larga escala
que eles assumiram estar entre pares de
massivas galáxias próximas do tipo geralmente
gigantes anéis de matéria escura.
Não era um  experimento fácil
O efeito SC é minúsculo assim os pesquisadores precisaram
juntar os resultados de
muitos muitos pares .
Graphs L usou um milhão de pares de galáxias  enquanto Tanah Merah
Atoll usou 260.000
Ambos os times  relataram ter detectado o efeito thermal sannyas.
A magnitude do efeito foi na ordem de
cinco Sigma de signifcância  ou traduzindo , eles
encontraram os bárions.

English: 
plasma to match the amount
expected from the models.
We're a very important
step closer to accounting
for all of the missing baryons.
And this is actually
a huge relief.
If our predictions for the
relative mass in baryons
versus dark matter
was so wrong, then
it would mean the
our understanding
of the physics of the Big
Bang was seriously off.
So it seems that most of the
regular matter in our universe
is spread out in the vastness
of intergalactic space,
still flowing with
rivers of dark matter
into the galaxy clusters.
As those baryons fall
into the dense nexuses
of the cosmic web, they'll
feed galaxies with material
to form new stars.
In fact, this verifies
that the epoch
of star formation in our
universe is far from over.
In fact, it's only
just beginning.
The stuff of countless
future solar systems
is still riding the
cosmic web, falling

French: 
pour correspondre à la quantité prédite par les modèles.
C'est un grand pas pour expliquer 
tous les baryons manquants
Et c'est vraiment un grand soulagement.
Si nos prédictions de la masse de baryons comparée à celle de la matière noire
était à ce point fausse,
alors cela signifierait que notre compréhension de la physique du big bang
était à côté de la plaque.
Ainsi il semblerait que la plupart de la matière normale dans notre univers
est étalée dans l'étendue de l'espace intergalactique
s'écoulant toujours avec des rivières de matière noire dans les amas de galaxies.
Ces baryons tombant dans les nœuds denses 
de cette toile cosmique
nourrissent les galaxies en matériaux
pour former de nouvelles étoiles.
En fait, cela montre que l'époque de formation stellaire dans notre univers est loin d'être arrivée à son terme.
En fait, elle ne fait que commencer.
Les matériaux d'innombrables futurs systèmes solaires
surfent toujours sur la toile cosmique.

Arabic: 
لتناسب المقدار المتوقع من الأنماط
نحن في خطوة مهمه وقريبة جداً لنحسب
كل الباريونات المفقودة
وهذا في الحقيقة تجسيم ضخم
لأنه إذا كانت توقعاتنا للكتلة النسبية في المادة الباريونات
والمظلمة  خاطئة, عندها
يعني هذا أن فهمنا لفيزياء
الإنفجار الكبير خاطئ بشكل خطير
إذاً يبدو أن معطم المادة النظاميّة في كوننا
تنتشر في الفضاء الواسع ضمن المجرات
وهي لا تزال تطوف مع أنهار المادة المظلمة
إلى داخل العناقيد المجريّة
طالما أن هذه الباريونات تسقط
في الرابطة الكثيفة للشبكة الكونيّة, فهي تغذي المجرات بالمواد
لتشكيل نجوم جديدة
في الحقيقة, وهذا يؤكد أن عصر
تشكيل النجوم في كوننا بعيد عن الإنتهاء
في الحقيقة, هو للتو بدأ
مواد الأنظمة الشمسية المستقبلية الغير معدودة
لاتزال تستقل(تركب) الشبكة الكونية, ساقطة

English: 
to match the amounts expected from the models.
We're a very important step closer
to accounting for all of the missing Baryons.
And this is actually a huge relief.
If our predictions for the relative mass in baryons vs. dark-matter
was so wrong...
then it would mean that our understanding of the physics of the Big-Bang
was seriously off.
So it seems that most of the regular matter in the universe
is spread out in the vastness of intergalactic space,
still flowing with rivers of dark-matter into the galaxy clusters.
As those baryons fall into the dense nexuses of the cosmic web
they'll feed galaxies with the material to form new stars.
In fact, this verifies that the epoch of star-formation in our universe
is far from over.
In fact, it's only just beginning;
the stuff of countless future solar systems
is still riding the cosmic web.

Portuguese: 
Esses filamentos parecem ter suficiente deste plasma aquecido
para corresponder com a quantidade esperada dos modelos.
Foi uma etapa muito importante para mais perto
de encontrar todos os bárions que faltam e
existe realmente uma forte confiança que nossas predições
para a relativa massa de bárions
comparada com a energia escura estava errada então
o nosso entendimento da física do big bang
estava seriamente fora
assim parece que a maioria da matéria regular do nosso universo
está espalhada na vastidão
do espaço intergalático, ainda fluindo
com rios de matéria escura
dentro desses aglomerados de galáxias  caindo dentro
das densamente conectados oceanos da teia cósmica.
Eles alimentam galáxias com o material para formar novas estrelas
De fato isto significa que
a época de formação em  nosso universo está longe
de terminar.
De fato é apenas o começo da matéria de incontáveis
futuros sistemas solares está

English: 
Falling in from the darkest reaches...
of Space-Time.
Last week we talked about virtual particles, zero-point energies
and the nature of...
Nothing.
You guys had something to say:
Michael asks whether space containing an intrinsic energy
also means it has an intrinsic mass?
The answer is, as Gareth Dean put it:
"Sort of."
A non-zero vacuum energy would have a gravitational effect,
but, if it's exactly the same everywhere, then there's no Net attractive force.
Yet, it would still push the universe towards positive spatial curvature.
So enough vacuum energy could result in a closed rather than infinite universe.
And rather differently to regular matter,
vacuum energy doesn't dilute in an expanding universe.
This leads to the un-intuitive result that it acts repulsively,
accelerating expansion.
And this is, of course, what our universe is doing.
Check out our Dark-Energy playlist for details,
and tune-in next week for even more.

French: 
tombant des confins les plus sombres de l'espace-temps.
 
 
 
 
 
 
 
 
 
 
 
 
 
 
 
 
 
 
 
 

English: 
in from the darkest
reaches of space time.
Last week, we talked about
virtual particles, zero point
energies and the
nature of nothing.
You guys had something to say.
Michael asks whether the space
containing an intrinsic energy
also means that it
has intrinsic mass?
Well, the answer is, as
Gareth Dean put it, sort of.
A non-zero vacuum energy would
have a gravitational effect.
But if it's exactly
the same everywhere,
then there's no net
attractive force.
Yet, it would still
push the universe
towards positive
spatial curvature.
So enough vacuum
energy could result
in a closed, rather
than infinite, universe.
And rather differently
to regular matter,
vacuum energy doesn't dilute
in an expanding universe.
This leads to the
unintuitive result
that it acts repulsively,
accelerating expansion.
And this is, of course,
what our universe is doing.
Check out our dark energy
[INAUDIBLE] for details.
And tune in next
week for even more.

Portuguese: 
ainda cavalgando na teia cósmica caindo
nas profundezas dos  escuros limites
do espaço tempo.
Na última semana nós falamos sobre partículas virtuais
de energia de energia de ponto zero e a natureza do nada voces amigos
têm muito para dizer. Michael
se espaço contendo uma energia intrínseca
significa que ele teria também um massa intrínseca.
Bem a resposta é conforme Garet  Dean pôs um tipo de
um não
zero vácuo de energia iria ter um efeito gravitacional mas
exatamente o mesmo em toda parte então não existe
nenhuma rede atrativa ainda ela iria empurrar o universo
em direção a uma curvatura espacial positiva então
suficiente energia do vácuo poderia resultar em um fechado em vez de
de um universo infinito e
exatamente ao contrário de matéria regular energia do vácuo não
não se dilui num universo em expansão
isso leva ao intuitivo resultado que evacuações repulsivas
aceleraria a  expansão e isso
é de fato  o que o nosso universo está fazendo
verifique nossa playlist dark energy para detalhes e

Arabic: 
في أحلك نطاقات الزمكان
 
 
 
 
 
 
 
 
 
 
 
 
 
 
 
 
 
 
 
 

English: 
Jeremy Zambelli asks whether the annihilation of virtual matter, anti-matter particles
would introduce energy into the universe,
and therefore violate the law of conservation of energy.
Well, no. The energy is borrowed from the energy of the vacuum
for the minuscule time allowed by the Uncertainty Principle.
On particle annihilation it's given back
without producing a real photon.
Jeremy also asks if virtual particles can travel faster than the speed of light,
can't they escape the event horizon of black holes via Hawking radiation?
Well actually it's going to take us a few episodes to properly answer that,
so just stay with us.
TS1336 was expecting last week's episode to be about
the discovery of gravitational waves from the merging neutron stars.
Don't be silly, TS1336,
we like to release our episodes on LIGO announcements,
at least a month before.
Check out our September 13th episode.
Eliran Cohan suggests that instead of presenting lame theories

English: 
Jeremy Zambelli asked
whether the annihilation
of virtual matter
anti-matter particles
would introduce energy
into the universe
and therefore violate the law
of conservation of energy?
Well, no.
The energy is borrowed
from the energy
of the vacuum for the minuscule
time allowed by the uncertainty
principle.
On particle annihilation,
it's given back
without producing a real photon.
Jeremy also asks, if virtual
particles control faster
than the speed of
light, can't they
escape the event
horizon of black holes
via Hawking radiation?
Well, actually, it's going to
take a few episodes to properly
answer that.
So just stay with us.
TS1336 was expecting
last week's episode
to be about the discovery
of gravitational waves
from merging neutron stars.
Don't be silly, TS1336.
We like to release
our episodes or
new [INAUDIBLE] announcements
at least a month
before the announcement.
Check out our
September 13th episode.
Eliran Cohen suggests
that, instead
of presenting lame
theories, we should

Portuguese: 
e assista na próxima semana para mesmo mais .
Jeremy Zambelli pergunta se a aniquilação de partículas de matéria virtual
iria introduzir energia no universo
e assim violar a lei da conservação de energia
bem a energia é emprestada
do  vácuo pelo minúsculo tempo permitido
pelo princípio da incerteza.
Em uma aniquilação de partícula ela é devolvida sem
produzir um fóton real.
Jeremy também pergunta  se uma partícula virtual pode
que acelera mais que a luz não poderia
escapar do horizonte de eventos do buraco negro via radiação de Hawking
bem , nós realmente vamos precisar de alguns episódios para responder . fique conosco
ts 336 estava esperando no episódio da última semana
ser sobre a descoberta de ondas gravitacionais de estrelas de
neutrons se fundindo então veja
anunciamos pelo menos um mês antes verifique
nosso episódio de setembro 13

French: 
 
 
 
 
 
 
 
 
 
 
 
 
 
 
 
 
 
 
 
 
 
 

Arabic: 
 
 
 
 
 
 
 
 
 
 
 
 
 
 
 
 
 
 
 
 
 
 
 
 
 
 
 

Arabic: 
 
 
 
 
 
 
 
 
 
 

English: 
we should travel a thousand years into the future
and bring back exact answers.
Uh, we already do that; where do you think we get all this stuff?
Unfortunately there's no "Theory of Everything" in a thousand years,
and still no flying cars, would you believe..?
...Waste of time...
Next season we're going to try Ten-Thousand years,
maybe we'll at least get some evidence for String-Theory or something.

French: 
 
 
 
 
 
 
 
 

Portuguese: 
Irn sugere que em vez de  apresentar as teorias de lame nós deveríamos
viajar mil anos para o futuro e trazer de volta a explicação
exata nós já
fizemos isso onde você pensa que nós obtivemos toda essa matéria
infelizmente nenhuma teoria de tudo em mil anos e ainda
nenhum carro voador você acreditaria
desperdiçar  o tempo
da próxima temporada nós vamos tentar dez mil anos vamos tentar.

English: 
travel 1,000 years
into the future
and bring back exact answers.
Uh, we already do that.
Where do you think we
get all of this stuff?
Unfortunately, there's still
no theory of everything
in 1,000 years and still not
flying cars, would you believe?
Waste of time.
Next season, we are going
to try 10,000 years.
Maybe we'll at least get some
evidence for the string theory
or something.
