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Galaxy Bias and the Evolution of Clustering

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L'Univers en évolution

4.6 (445 notes) | 48K étudiants inscrits

This is an introductory astronomy survey class that covers our understanding of the physical universe and its major constituents, including planetary systems, stars, galaxies, black holes, quasars, larger structures, and the universe as a whole.

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4.6 (445 notes)

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JI

Apr 28, 2019

I really enjoyed every lesson. It's an incredible and very complete course. Anyone who loves astronomy should do it. In addition, I was able to improve English, which is my second language.

AH

Oct 19, 2015

Took this professor's course in Galaxies and Cosmology which was for 2nd year physics majors. I think this course is a more general course for non-physics-majors. Excellent course!

À partir de la leçon

Week 8

Large Structure11:08

Quantifying Large Scale Structure: Galaxy Correlations and Power Spectrum7:48

The Large Scale Velocity Field8:20

Galaxy Bias and the Evolution of Clustering7:30

Structure Formation: The Growth of Density Perturbations11:21

Galaxy Clusters10:35

Enseigné par

S. George Djorgovski
Professor

Transcription

So let's now see how is clustering evolving in the universe.

And that introduces a interesting phenomenon called Galaxy Biasing in

which I hinted already.

And what's meant by this is exactly what we implied,

that you can observe structures in light,

some differential density amount, access sort of efficiency divided by the mean.

So the relative variations in density of light,

are somehow related to the relative variations in density of mass.

And the simplest thing to say is there is just direct proportionality,

and if constant is equal to one then they're fair tracer.

So that little constant b is called the bias factor, and it turns out that,

in fact, b squared is the number that connects the observed

two-point correlation function with the light with that of the underlying mass.

So because b could be different, like if galaxies

are clumped more strongly than the mass, b will be greater than 1.

That's what proportionality is, right?

And say b is 2 or 3 or 5, then galaxies would not be a fair tracer of mass.

They'd be a biased tracer of mass.

They would be favoring the densest spots.

And so that was the basic idea.

And turns out that some of that is actually happening.

And the simple model for this is let's assume that in very distant universe,

wen you start forming galaxies, you require them to be above

certain density threshold for stuff to fall together and ignite star formation.

Now remember density field can be

interpreted as a superposition of waves of different wavelengths and amplitudes.

So you have small waves riding atop of large waves.

Now if you impose a threshold, then you're naturally going to select first

the small peaks that are riding on top of big waves.

And so in this picture, first galaxies were formed

in first clusters, and then star formation was spread out.

An equivalent of that would be, say,

if you look at the snow line on planet Earth, right?

You will see that it's only the peaks of the highest mountains that are covered.

Or, even if you are just to say, let's ask where is this Earth's surface is

a function of elevation, but first you see just whole bunch of correlated spots,

Andes, and Rocky Mountains, and Himalayas.

And then as you lower down the threshold,

eventually all the surface area of the earth is encompassed.

So with galaxy formation the idea is that you start with the densest spots and

then eventually spread further out as you get more time.

And this is an illustration of this from a numerical simulation,

onto this simulation's of structure formation

showing both what gas and stars do and what the dark matter does.

And people who did simulation know exactly where the particles are,

and then they asked, okay, what are the 1-sigma deviations from the mean, and cut,

what are 2-sigma, 3-sigma, then they run out of volume.

And you can see the higher threshold of contrast you demand,

the more clustered will those spots be.

So this also explains why clusters of galaxies

are clustered more strongly than galaxies themselves,

which was very puzzling until Nick Kaiser came up with this idea.

All right, so does bias depend on something?

Well, remember two-point correlation function was different for

bright galaxies and faint galaxies, and red and blue and

so on, and that is simply reflecting the bias factor.

The more luminous, more massive galaxies are higher bias factor so

they look more strongly correlated.

And so this has now been measured and seems to fit theoretical models just fine.

Okay what about evolution in time?

Well generically, you expect that clustering grows stronger in time,

because the density field slowly collapses upon itself.

Galaxies, coagulate, they creep more.

So you expect that there is less clustering in the past than there is

here now.

All right, so

you expect a weaker clustering at larger edges as you go far away.

And, sure enough, that is what you see.

This is plot of the strength of correlation function on the sky as

a function of depth and survey.

And the deeper you go, the weaker it gets.

This is what you generally expect.

And this goes all the way out to about when Euros was half it's present size.

But then beyond that, something weird happens, it turns around.

Then as you go deeper in the past, clustering seems to grow stronger.

Which makes no sense whatsoever,

because you couldn't just collapse things, and then let them fly apart.

So how is this possible?

And the answer is the bias itself evolves.

This was already sensed in these redshift histograms from deep pencil beams surveys.

I told you how it seemed to be encountering the same type of structures

no matter how far we go, filaments and so on.

And now we think we know why this is.

And so look at this.

[SOUND] Consider, say just behavior of

the highest contrast fluctuations,

5- sigma fluctuations.

Those will be the densest, and they will start collapsing first.

And those will be the first one to turn on galaxy formation.

Then you go to lower threshold, say 3-sigma fluctuations.

They'll be following but with some time delay.

And so on down to lowest fluctuations.

So if you impose a threshold, then the high speeds

would reach it first, and those are beyond the galaxies that you can see.

So because those are the most biased spots in the density field,

you'll see that galaxy clustering was stronger in the past.

Instead of that, you're not actually seeing behavior gambling mass for

underlying mass the all growing time, only growing time.

But the illuminated peaks which ones, that changes.

And that explains the observations.

And so now we can ask the question,

how is that evolving in time again from very deep surveys.

And you can see that near us, at low rated bias factor is about one.

Just as I told you before.

But then as you keep going to higher and higher arches, it keeps climbing.

And in fact when time galaxies were forming, maybe 5-sigma peaks or

6-sigma peaks were the ones to first go non-linear and ignite.

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