Transcriber: Tijana Mihajlović Reviewer: Ilze Garda
When I was a PhD student, which was actually not so long ago,
we only had a vague idea
about the history and the composition of our universe.
There was still a lot of room for speculation on various ideas.
But since then, we, cosmologists,
have experienced a burst of new observations and discoveries
over the range of just 20 years.
We now understand several details
about the history of our universe over the past 13 billion years.
And believe me,
it has been terribly exciting to be part of a generation of physicists
that, at a unique moment in the history of mankind,
have been able for the first time, on a reliable basis,
to understand what our universe looks like on very large scales.
Humans have been making assumptions about that since ever,
but the actual reality of our universe has been unveiled to us
precisely over the past two decades.
And for me, this is astonishing.
So let me illustrate more concretely
what I mean when I say that we now understand our universe.
For instance, these two pies show, at two very different moments,
the cosmic recipe,
that is, the composition of the universe in terms of different particles,
like atoms, neutrinos, dark matter, et cetera.
What is remarkable
is that we are able to pinpoint the amount of each of these ingredients
with a precision of a percent,
despite the fact that most of these species
cannot leave any track in our detectors,
and despite the fact that the universe is, of course,
far too big for sending detectors all around.
This is a bit as if by observing a cake and not even tasting it,
we could tell its recipe with percent precision.
Second example.
This chronology shows that our universe over the past 13 billion years
went through four different stages,
each of them with extremely different properties.
During the first stage, our universe was very dense,
very homogeneous and in an ultrafast expansion.
During the second stage,
the whole universe was extremely hot and bright
- a bit like the interior of a star, everywhere -
and the expansion started to slow down.
During the third stage, everything became cold and dark,
and the first galaxies formed, separated by huge regions of empty space.
Finally, during the fourth stage,
the expansion of the universe started to accelerate again.
Amazingly, we have very strong proofs
that each of these epochs really occurred,
and we can even date them with high precision.
So, the fascinating question that I want to address today is:
but how could we understand all these details from our tiny planet?
And how can we be so sure,
while hundreds of generations before us have tried to reach this knowledge
without being able to go beyond the level of assumptions or beliefs?
The answer is connected to the word "spectrum".
We understand all this
because we have been able to measure the spectrum of the universe.
A spectrum is a quantity used by scientists
to describe anything in nature
that vibrates, or fluctuates with time, or varies over space,
like any sounds, or any lights, or any image.
The spectrum is the decomposition of the sound, of the light, of the image
into various frequencies or wavelengths.
So, for instance, any sound has its own spectrum.
To show it, let me open on my laptop
a sound analyzer
- that's it - and just blow this flute.
(Flute sound)
OK, that's it.
On the right, you see the spectrum of the sound that we just heard,
and each music instrument has its own spectrum.
Even two flutes or two violins can be distinguished
through tiny differences in their spectrum,
so the spectrum is really like the fingerprint of a given sound.
But what goes for a sound also goes for an image.
Here is a famous painting, "The Garden of Earthly Delights".
This image can be decomposed
into a sum of patterns of different frequencies,
and the spectrum is just the amount of each frequency or wavelength.
So, for instance,
here is the spectrum of wavelengths in this particular image.
Again, it's like the fingerprint of the image.
What is fascinating
is that we are able to do the same for the whole universe.
We can define its spectrum,
and, since a few years, we are even able to measure it.
So now I want to explain and show you
the holy grail of cosmology,
the quantity that we were grimming to observe when I was a PhD student:
His Majesty the Spectrum of the Universe.
But before that,
let me recall that when we point a telescope in a given direction,
we collect light from various distances,
and the farthest that light is,
the farthest back in history we can see.
And if with the telescope
we select the light coming from the farthest possible distance,
then we start to see a very special type of radiation,
a leftover from the Big Bang, called the cosmic microwave background.
It has been first observed in the 60s, bringing a Nobel Prize.
But after this first discovery,
scientists asked themselves a question:
is this microwave background exactly the same in all directions?
And it turns out that it is nearly the same,
but with small fluctuations.
This radiation can be a bit more intense in a given direction
and a bit less in another direction.
Since the 70s,
cosmologists have tried to establish a map of these fluctuations,
and it has been a very difficult task.
The first map has been obtained 22 years ago
by the COBE satellite from NASA.
On this map,
different colors indicate slightly different levels of intensity
in the cosmic microwave background.
This is a map of the full sky
that has been unfolded and projected over an ellipse,
like we would do with a more usual map of stars and constellations.
The problem with the COBE map was its poor resolution,
the fact that it is very fuzzy.
For comparison, imagine that we look at the same painting as before,
but from very far away with a telescope having a limited resolution.
Then, we might see a very blurry image like this one,
and in order to understand what the image is really about,
we would need to increase the resolution of the telescope like this.
Well, it had been exactly the same with the COBE map.
Several experiments have tried to measure it with better resolution.
The most recent and precise experiment
has been the Planck satellite from the European Space Agency.
It has recently produced this exquisitely precise map.
The COBE instruments have been already using amazing technology,
but to produce such a high resolution and high sensitivity map,
it was necessary to use detectors, about 1,000 times more sensitive,
so this is really relying on the best cutting-edge human technology.
And from that map, it is possible to get a spectrum.
I promised that I would show you His Majesty the Spectrum of the Universe.
Well, here it is.
These red dots are what we consider
as the fingerprint of our universe.
It could only be measured very recently
thanks to exquisite experiments like Planck.
But in science it’s not enough to have fantastic observations.
Alone, this spectrum is not telling us anything about the universe.
To make it speak, we need to confront it to a theory.
In fact, in science, every time that theories match observations,
we learn something new.
Actually, over the 20th century, lots of theories have proposed
various possible models to describe our universe,
relying on their understanding of the laws of physics,
but not yet on precise observations like this one.
Later, in the 90s, we started to develop
some numerical codes able to simulate the evolution of the universe
in each of these models.
Actually, one such code is installed on my laptop.
To use the code, you need to start from a possible model of the universe,
then you press a key, and the computer will simulate
13 billion years of cosmological evolution
in only about one second.
And after that, it will compute
the spectrum of the universe in this particular model.
So, let’s play this game together.
I turn on the code,
and I start from some assumptions from a given model for the universe
with some numbers describing the composition of the universe
in that model and some other properties.
Then I press a key,
and that’s it.
The laptop has simulated 13 billion years of evolution
and has computed the spectrum of this model.
Now we can compare it with the true observed spectrum.
We find a complete mismatch,
showing that we actually started from a very bad guess.
But we can try other models.
And we, cosmologists, have played this game
over the last years in a systematic way, trying billions of simulations,
and we could establish that there is one model
leading to perfect agreement with observations.
Let’s simulate it now.
I go back to this code,
and now I will run with the new assumption
in which the cosmic pie is actually exactly the same
as we have seen in the second slide.
I start the simulation, and I get this new spectrum
that I can now compare to the true observed one,
and the agreement is beautiful.
Moreover, we know that there is no alternative model
significantly different from this one which gives such a good fit to the data.
So this is exactly the way in which we have been able to understand
all these details about the composition and the history of the universe.
The research in this field keeps going.
As you can see, we now understand the big picture,
but there are still some details requiring further investigation.
For instance, I showed you these four stages
in the evolution of the universe.
We can date precisely the last three stages,
but there is still a big uncertainty concerning the time
at which the first stage, called inflation, ended up.
However, measuring this time will have very deep implications for physics.
Actually right now,
the measurement of this time is a topic of big controversy
between different experiments on both sides of the Atlantic,
and the answer might come in maybe a few months, if we are lucky,
from new observations.
So stay tuned about new discoveries in cosmology
and, please, enjoy the privilege to belong to the first generation of humans
who understand the secrets of our universe.
Thank you.
(Applause)