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.

Loading...

From the course by Caltech

The Evolving Universe

361 ratings

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.

From the lesson

Cosmology and the Deep Universe

- S. George DjorgovskiProfessor

Astronomy

Let's talk about supernova standard candles, and

how do we use them in the Hubble Diagram.

Supernovae bright.

This is really what makes them useful for cosmological measurements.

And you recall there are two types, Ia, which are detonating white dwarfs,

and Type 2 which are thermonuclear bombs of massive stars.

It turns out that it this Type Ia can be used as standard candles.

By themselves, the peak brightness of Ias has a substantial scatter.

But it turns out that that scatter correlates with the width

of the light curve, how long it takes the supernova to get brighter and dimmer.

And when you correct for that effect, you get superb,

almost constant standard candle, to better than 10%.

And it looks like this.

So the light curves on top,

there's a whole bunch of independently measured ones.

And then, you can see that there is a spread, both in width and

in the amplitude.

So you correct for the spread in the amplitude by using function of the width.

And suddenly, they all collapse onto one standard candle light curve.

Since the width is something that does not depend on cosmology,

it's just, follow the light curve, you can measure that.

You can correct the observed light curve and compare it to what you got here.

So this was actually very transformative measurement.

First it was done to figure out what Hubble constant was,

but then it was carried out into far field cosmology.

And this is what it looks like.

The top diagram shows you, if you just plot peak brightness

of a type Ia supernova, whereas this redshift, the other way.

There is considerable scatter.

You make a correction, and the scatter goes down to measurement errors.

Beautiful.

So for nearby supernovae, relatively nearby, you get Hubble Diagram.

This is now log redshift, log velocity, vs log of flux.

And it's almost perfect straight line.

So locally, you can use this to measure the expansion rate,

the slope of this line.

Then as you go to higher redshifts, meaning larger load peak times,

cosmic geometry effects come in, and possibly illusionary effects.

So two groups, in 1998, the Supernova Cosmology Project and

High Redshift Supernova Team, did this.

They used nearby sample supernovae to anchor their Hubble diagram.

Then they looked at the very distant ones.

And the idea here is that a priori, the spot would be standard candle because it

depends on fundamental physics of stellar evolution, Chandrasekhar Mass.

And that's what makes them standardized.

If you push over Chandrasekhar Limit, thing explodes.

And that's been tested, and actually is a good assumption.

And so they got really high precision Hubble diagrams.

And they both found the same thing, that the best fit models for

supernovae, Hubble [INAUDIBLE] standard candles imply the existence

of cosmological constant.

They tried every kind of correction, anything you can think of,

to get rid of this, and they just couldn't find it.

All the selection effects going the other way, right?

Remember, all models with cosmological constant make things look dimmer.

So it's not like you're losing them, if they're found the opposite effect,

they you only see the bright ones,

then you worry about selection effect that pushes you in the opposite direction.

So this result has stood the test of time.

Many groups have done this now, with many, many more objects.

And everybody gets the same result.

So that's very encouraging.

So the leaders of the two groups, Riess and Schmidt on one side,

and Perlmutter on the other, shared a Nobel prize for physics and

well deserved, I should say.

There is a lot of interesting background stories to this,

which I will not tell you.

But it was really a milestone that finally,

physicists understood that there is such a thing as cosmological constant.

And this is today, one of the major outstanding mysteries of physics.

So this is what happens when you plot these things

on the normal RFT diagram, inverting Hubble diagram back.

And so all of the observed data points are now in the past,

telling them what curve we sit, and extrapolate to the future.

And essentially, it says the universe is open, and it will expand forever.

Well, it's flat, but it will expand forever.

And this is fairly recent version.

Just couple years old.

We can see now there are many, many,

many more data points have been added, and the results have been holding up.

And now we see supernovae with Hubble space telescope all the way to

about redshift one and a half, and everything works beautifully.

Coursera делает лучшее в мире образование доступным каждому, предлагая онлайн-курсы от ведущих университетов и организаций.