Unser Universum: COSMO-19, RWTH Aachen 5. September 2019 Der - - PowerPoint PPT Presentation

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Unser Universum: COSMO-19, RWTH Aachen 5. September 2019 Der - - PowerPoint PPT Presentation

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ffentlicher Vortrag Unser Universum: COSMO-19, RWTH Aachen 5. September 2019 Der Anfang und ein Ende Eiichiro Komatsu Max-Planck-Institut fr Astrophysik We have seen the beginning of the Universe, using this space telescope called

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Öffentlicher Vortrag COSMO-19, RWTH Aachen

  • 5. September 2019

Unser Universum: Der Anfang — und ein Ende Eiichiro Komatsu

Max-Planck-Institut für Astrophysik

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We have seen the beginning

  • f the Universe, using this

space telescope called “WMAP”

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We have seen the beginning

  • f the Universe, using this

space telescope called “WMAP”

I am serious!

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WMAP is a parabola antenna

Parabola antenna

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June 30, 2001: WMAP was launched on the Delta 2 rocket from Cape Canaveral, Florida, USA

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WMAP leaves Earth

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WMAP goes beyond Moon!

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1.5 million kilometers from Earth

WMAP circles around the “Lagrange 2 Point”

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WMAP observes the Universe with Sun, Earth and Moon being behind

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Seeing the beginning?

  • Looking into the distance = Looking into the past
  • The sun light takes 8 minutes to reach Earth
  • The next nearest star is 4 light years away
  • The next nearest galaxy is 2.5 million light years away
  • Und so weiter
  • You keep looking farther away, and eventually reach

the beginning of the Universe!

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WAS?!

  • I am sure that some of you thought that I am crazy
  • Today’s goal: I will convince you that

“Komatsu is not crazy, but he is

saying something real. We can really see the beginning of the Universe!”

  • In my lecture, you will be hearing well-established results

from a series of observations and measurements made

  • ver the last half century
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Fireball Universe

Hot and Dense

Time Space

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Hot and Dense Hot

Expansion Fireball Universe

Time Space

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Hot Cooled down Hot and Dense

Expansion Expansion Fireball Universe

Time Space

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Definitive Result

  • Those photons which filled the fireball Universe are

still with us

  • There are 410 such photons

per cubic centimetre

  • These photons are pouring on us all the time!
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Sky in the visible light [~500nm]

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Sky in the microwaves [~1mm]

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Sky in the microwaves [~1mm]

Light from the fireball Universe filling our sky The Cosmic Microwave Background (CMB)

Die kosmische Mikrowellenhintergrundstrahlung

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Full-dome movie for planetarium Director: Hiromitsu Kohsaka

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Wavelength of Light

Wavelength Wavelength

  • Visible light is
  • shorter wavelength
  • 380–740 nanometers
  • Microwave is
  • longer wavelength
  • millimeter to centimeter
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All you need to do is to detect micro

  • waves. For example, 1% of noise on

the TV is from the fireball Universe

  • Dr. Hiranya Peiris

（University College London）

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１９６５

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1:25 model of the antenna at Bell Lab The 3rd floor of Deutsches Museum

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The real detector system used by Penzias & Wilson The 3rd floor of Deutsches Museum

Donated by Dr. Penzias, who was born in Munich

Arno Penzias

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Recorder Amplifier Calibrator, cooled to 5K by liquid helium

Horn antenna

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May 20, 1964 CMB Discovered

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6.7–2.3–0.8–0.1 = 3.5±1.0 K

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Spectrum of CMB = Planck Spectrum

4K Planck Spectrum 2.725K Planck Spectrum 2K Planck Spectrum Rocket (COBRA) Satellite (COBE/FIRAS) Rotational Excitation of CN Ground-based Balloon-borne Satellite (COBE/DMR)

3mm 0.3mm 30cm 3m

Brightness Wavelength

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１９８９ COBE

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The sky in various wavelengths

Visible -> Near Infrared -> Far Infrared -> Submillimeter -> Microwave

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２００１ WMAP

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WMAP Science Team

July 19, 2002

  • WMAP was launched on June 30, 2001
  • The WMAP mission ended after 9 years of operation
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2001 WMAP

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Our Origin: Tiny fluctuations in the early Universe

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A Remarkable Story

  • Observations of the cosmic

microwave background and their interpretation taught us that galaxies, stars, planets, and ourselves originated from tiny fluctuations in the early Universe

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Some of the findings

  • We determined the age of the Universe
  • 13.8 billion years
  • We determined the composition of the Universe
  • What is the Universe made of?
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Kosmische Miso Suppe

  • When matter and radiation were hotter than 3000 K,

matter was completely ionised. The Universe was filled with plasma, which behaves just like a soup

  • Think about a Miso soup (if you know what it is).

Imagine throwing Tofus into a Miso soup, while changing the density of Miso

  • And imagine watching how ripples are created and

propagate throughout the soup

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Outstanding Questions

  • Where does anisotropy in CMB temperature come

from?

  • This is the origin of galaxies, stars, planets, and

everything else we see around us, including

  • urselves
  • The leading idea: quantum fluctuations in

vacuum, stretched to cosmological length scales by a rapid exponential expansion of the universe called “cosmic inflation” in the very early universe

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  • Decompose temperature

fluctuations in the sky into a set of waves with various wavelengths

  • Make a diagram showing the

strength of each wavelength

Data Analysis

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Long Wavelength Short Wavelength

180 degrees/(angle in the sky) Amplitude of Waves [μK2]

WMAP Collaboration

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Long Wavelength Short Wavelength

Measuring Abundance of H&He

Amplitude of Waves [μK2]

180 degrees/(angle in the sky)

Fraction of H&He

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  • WMAP determined the

abundance of various components in the Universe

  • As a result, we came to

realise that we do not understand 95%

  • f our Universe…

H&He Dunkle Materie Dunkle Energie

Cosmic Pie Chart

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Matter and Expansion

  • How would space expand in an empty Universe?

–A: Continue to expand with a constant velocity (i.e., no acceleration or deceleration)

  • How would space expand in a matter-dominated Unvierse?

–A: Gravity pulls space and expansion decelerates

  • Too much matter means a re-collapse of the Universe!

Big Bang Big Crunch

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Accelerating Universe

  • However, the observations tell us that expansion is speeding up!
  • This cannot be due to matter

–Something that is not even matter: Dark Energy Big Bang

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No Dark Energy on Earth

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What if Dark Energy dominates?

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Dark Energy determines the future of the Universe

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Future of the Universe

  • It all depends on what Dark Energy will do!
  • We are “safe” in Earth because there is a lot more

matter than Dark Energy on Earth today

  • If Dark Energy stays the same or decreases in the future,

we will be safe forever

  • If Dark Energy increases over time, it will eventually

exceed the matter density, and everything will be ripped

  • apart. A catastrophic ending called “Big Rip”
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Big Rip

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Der Anfang, und ein Ende

  • Our origin: tiny fluctuations in the early Universe
  • How were we born? See it by yourself in the last

scene of the movie “HORIZON”

  • And remember from today: We are always

surrounded by the light from the beginning of the Universe!

  • Finally, all of this research has been made possible by

tax payer’s money. We are always very, very grateful to your support. Vielen Dank für Ihre Unterstützung und Ihr Zuhören!

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