All language subtitles for Black Hole Apocalypse PBS Nova 720p HDTV MVGroup EN Sub

♪ ♪

JANNNNA LEVIN:
Of all the objects
in the cosmos...

Planets...

Stars...

Galaxies...

(explosion echoes)

LEVIN:
None are as strange,

mysterious,

or powerful

as black holes.

♪ ♪

NEIL DEGRASSE TYSON:
Black holes are

the most mind-blowing things
in the universe.

PRIYAMVADA NATARAJAN:
They can swallow a star

completely intact.

FERYAL OZEL:
Black holes have
these powerful jets

that just spew matter out.

LEVIN:
First discovered on paper...

PETER GALISON
On the back of an envelope,

some squiggles of the pen.

LEVIN:
...the bizarre solution

to a seemingly
unsolvable equation...

A mathematical enigma...

LEVIN:
Einstein himself

could not accept black holes
as real.

People didn't even believe for
many years that they existed.

Nature doesn't work that way.

♪ ♪

LEVIN:
Yet slowly, as scientists
investigate black holes

by observing
the effect they have

on their surroundings,

evidence begins to mount...

ANDREA GHEZ:
That is the proof
of a black hole.

TYSON:
Millions of times
the mass of the sun.

LEVIN:
Cutting-edge discoveries show...

We did it!

(applause)

LEVIN:
...black holes are very real.

I thought it was crazy.

I said, "Holy (bleep)!"

♪ ♪

LEVIN:
But what exactly are they?

If we could visit one,
what might we see?

With their immense power,
do black holes somehow shape

the very structure
of the universe?

Is it possible we might
not exist without them?

It's quite a journey.

♪ ♪

LEVIN:
"Black Hole Apocalypse."

Right now on "NOVA."

♪ ♪

VIN:
There are apocalyptic objects
in the universe:

engines of destruction,

menacing and mysterious.

Black holes.

Even scientists
who study them

find them astonishing.

EILAT GLIKMAN:
Black holes can sort of
blow your mind.

I'm amazed that these objects
actually exist.

LEVIN:
Black holes defy
our understanding of nature.

Black holes are the greatest
mystery in the universe.

LEVIN:
They're completely invisible,

yet powerful beyond imagining.

They can tear a star
to shreds.

OZEL:
Black holes actually

will eat anything
that comes in their path.

You really want to avoid them
at all cost.

LEVIN:
Black holes even slow time.

Once thought too strange
to be real...

(glass shatters)

...black holes shatter our very
understanding of physics.

But we're learning they may
somehow be necessary

for the universe we know
to exist.

They might well be the key
players in the universe.

LEVIN:
What are these strange,
powerful objects,

outrageous and surprising?

Where are they, and how
do they control the universe?

The search for black holes
is on.

And it will be a wild ride
across the cosmos

to places where everything you
think you know is challenged --

where space and time,
even reality,

are stranger than fiction.

♪ ♪

And we're starting that journey
at a very unlikely place:

here, at a remote location
in Washington state,

where-- for the first time--

a radical new experiment
has detected black holes.

It originated over 50 years ago,

when a few visionary scientists

imagine a technology
that hasn't yet been invented...

♪ ♪

Searching for something
no one is certain can be found.

The experiment
is daring and risky.

Failure could mark
their lives forever.

But they don't fail.

Right here, in these facilities,

they make
a remarkable discovery.

In the early hours
of September 14, 2015,

they record a message.

It looks and sounds like this.

(chirp)

Just a little chirp.

But that chirp is epic,
monumental.

The signal traveled over a
billion light years to reach us.

♪ ♪

It started far, far away.

And what it tells us is this:

somewhere in the cosmos,
over a billion years ago,

two massive black holes circle
each other in a fatal encounter.

Closer and closer they come,

swirling faster and faster,

until finally,
they slam together.

(drum beats)

The black holes create waves
that spread outward.

(drum beats)

Just like vibrations on a drum,

a ringing in the fabric
of space itself.

The collision creates
a massive blast,

putting out 50 times
as much power

as the entire visible universe.

It sends out a wave not of heat,
or light, or sound,

but of gravity.

This gravity wave is moving
its way through the universe

at the speed of light.

♪ ♪

LEVIN:
The wave races by stars.

On the young Earth,
supercontinents are forming.

Microscopic organisms
have just appeared.

TYSON:
Washing over one galaxy

after another, after another.

LEVIN:
Dinosaurs roam the Earth.

The wave is still moving.

LEVIN:
It zooms through clouds of dust.

And then it nears
the Milky Way Galaxy.

LEVIN:
The Ice Age is just beginning.

We're troglodytes,
drawing in caves.

LEVIN:
The wave reaches nearby stars.

Albert Einstein is
in the sixth grade.

The wave approaches as close
as Alpha Centauri.

At midnight
on September 13, 2015,

it is as close as Saturn.

Finally, over a billion years
after the black holes collide,

the wave reaches us.

It strikes a pair

of revolutionary new
observatories--

the sites of
the daring experiment.

(faint chirp)

This is LIGO,

the Laser Interferometer
Gravitational Wave Observatory.

The experiment
50 years in the making

has finally hit the jackpot--

and opened an entirely new way
of exploring the universe.

For 400 years, almost everything
we've observed in space

has come to us in some form
of electromagnetic energy.

(chirp)

That little chirp is different.

What hits the Earth
in September 2015

is a gravitational wave--

a squeezing and stretching
of the very fabric of space.

It produced no light;

no telescope could ever see
the collision.

We needed an entirely new kind
of observatory to detect it.

That wave is new
and direct evidence

of one of the strangest
mysteries in our universe:

black holes.

♪ ♪

Most of us have heard
of black holes.

They're invisible, powerful...

NATARAJAN:
We are talking about things

that are a billion times
the mass of the sun.

LEVIN:
Bizarre.

GLIKMAN:
A physical entity

with infinite density.

No beginning, no end.

LEVIN:
They pull things in.

And warp light.

Approach one, and time itself
begins to change.

NATARAJAN:
The gravity is so intense
that a moving clock

will tick slower.

TYSON:
Time will become so slow for you

that you will watch the entire
future of the universe

unfold before your very eyes.

LEVIN:
Fall in, and you'd be squeezed
as thin as a noodle.

TYSON:
You'll be extruded through
the fabric of space and time

like toothpaste through a tube.

♪ ♪

LEVIN:
Today, we know more about
black holes than ever before.

But the more we learn,
the more mysterious they become.

GHEZ:
They're the most exotic objects
in the universe.

We don't have the physics
to describe them.

NATARAJAN:
No matter how well
you understand them,

they remain unreachable
in some sense.

ANNOUNCER (on film):
Now man is about to enter...

the black hole!

(machine beeping)

So black holes have
a pretty fierce reputation.

And if you want a villain for a
sci-fi movie, cast a black hole.

But in reality, what exactly
is a black hole?

And where do they come from?

You might think a black hole
is like this-- an object.

But it's not.

It's a hole
in the fabric of space.

A place where there is nothing;
nothing except gravity,

gravity at its most intense
and overwhelming.

♪ ♪

So if black holes are
all about gravity--

gravity at its most extreme--

what exactly is gravity?

♪ ♪

(bell rings)

(people chatting)

We're all familiar
with gravity.

(plates crash):
Yep, it's Friday.

LEVIN:
It rules our lives.

But even so,
for a very long time,

how gravity actually works

was one of
the greatest mysteries.

Over 300 years ago,

Isaac Newton was fascinated

with the behavior
of moving objects.

Eventually he figured out
his laws of motion.

They work so well,
we still use them today.

MAN (on film):
Lift-off, we have lift-off
at 9:34 a.m.

But Newton's laws can only
describe gravity's effects,

not explain what it is.

NEWTON (dramatized):
Hm.

And here's where
Albert Einstein comes in.

(camera clicking)

Like Newton, he thinks
about objects in motion.

And he wonders
what gravity actually is.

Is it a force?

Or could it be something else?

Here's what concerns Einstein.

Take this apple.

I can't move it
without touching it.

But if I drop the apple,
it moves toward the Earth.

But what if I take my hand away,

and the floor, and the basement,
and the floor below that?

Then what happens?

The apple just keeps falling.

Einstein realized that gravity

had something to do
with falling.

Now, if I throw the apple,

it falls along a curved path.

But imagine I could get the
apple moving much faster.

(cannon firing)

Eventually, if I get the apple
moving really, really fast--

say, 17,000 miles an hour--

its curved path matches
the curve of the Earth.

The apple is in orbit,
falling freely,

just like the International
Space Station

and the astronauts inside it.

According to Einstein,
the apple--

and the space station,
and the astronauts--

are all falling freely
along a curved path in space.

And what makes that path curved?

The mass of the Earth.

GALISON:
Einstein came up with
a supremely simple concept,

and that is that space and time
is bent by the Earth,

and by the sun, and by
all the objects in the world.

So according to Einstein,

the mass of every object causes
the space around it to curve.

GALISON:
And that was
Einstein's conception.

There are no forces anymore.

There's just objects
bending space-time

and other objects following
the straightest line through it.

LEVIN:
All objects in motion
follow the curves in space.

So how does the Earth move
the apple without touching it?

The Earth curves space,

and the apple falls freely
along those curves.

That, according to Einstein's
general theory of relativity,

is gravity: curved space.

And that understanding
of gravity--

that an object causes the space
around it to curve--

leads directly to black holes.

But it's not Albert Einstein
who first makes the connection

between gravity
and black holes.

It's another scientist.

MARCIA BARTUSIAK:
Karl Schwarzschild

was a German astronomer,

head of the Potsdam Observatory
in Germany.

Ever since he was a teenager,
he had been calculating

complicated features
of planetary orbits.

LEVIN:
As Einstein unveils his theory
of gravity in 1915,

Karl Schwarzschild
is in the German army,

calculating artillery
trajectories in World War I.

BARTUSIAK:
And just weeks after Einstein
presented his papers,

Schwarzschild,
then on the Russian front,

quickly got a copy
and was mapping

the gravitational field
around a star.

GALISON:
Einstein had gotten at it

through a series
of approximations.

But Schwarzschild,
sitting on the front

with bullets and bombs flying,

calculated an exact solution
to Einstein's theory

and sent it to Einstein.

Einstein was astonished.

He hadn't even imagined

that you could solve
these equations exactly.

LEVIN:
But Schwarzschild isn't done.

In his solution
to Einstein's equations,

he discovers something Einstein
himself had not anticipated.

GALISON:
Schwarzschild said,

"I can calculate
this strange distance

"from a gravitating object

that represents
a kind of boundary."

LEVIN:
Schwarzschild mathematically
concentrates a mass--

for example, a star--

into a single point.

Then he calculates how that mass
would bend space

and curve rays of light
passing nearby.

BARTUSIAK:
As he, through his mathematics,

aimed particles of light
or matter towards this point,

there was this boundary
surrounding the point

at which the particles
would just stop.

The particles disappeared.

Time stopped.

LEVIN:
Schwarzschild has discovered

that a concentration of mass
will warp space

to such an extreme

that it creates a region
of no return.

Anything that enters that region
will be trapped,

unable to escape-- even light.

GALISON:
It's like those roach motels.

You can check in,
but you can't check out.

Once you go
across that boundary,

even if you can sail through,

there's nothing you can do
to get out,

there's nothing you can do
to signal out.

It becomes this strange,
cut-off portion of space-time.

LEVIN:
What Karl Schwarzschild has
discovered is that any mass,

compressed
into a small enough space,

creates what we today
call a black hole.

But Albert Einstein--

whose own theory of gravity
predicts such a thing--

cannot believe it can happen
in the real world.

BARTUSIAK:
Einstein didn't think

that nature would act like this.

He didn't like this idea.

LEVIN:
Karl Schwarzschild becomes ill
and dies before he has a chance

to further investigate
his own discovery.

(crowd cheering)

LEVIN:
Two-and-a-half years later,
in November 1918,

World War I ends.

The strange theoretical sphere
discovered by Karl Schwarzschild

seems destined to be forgotten--

nothing but
a curious historical footnote.

(explosion echoes)

But in the coming decades,

physicists learn more
about the atom

and about how fusing atoms
powers stars--

a process called nuclear fusion.

Some begin to wonder
if something like a black hole

could actually come from a star.

But not just any star--
it would have to be big.

GLIKMAN:
Stars are born in litters,

and you get a distribution
of sizes and masses;

thousands of little stars

and a few big stars,
very big stars,

incredibly massive.

NIA IMARA:
Stars are in many ways similar
to living creatures.

Like humans,
they have life cycles.

LEVIN:
Investigating stars' life cycles
in the 1930s, two visionaries--

Subramanyan Chandrasekhar
and Robert Oppenheimer--

discover
that the most massive stars

end their lives very differently
from smaller ones.

The life cycle of a star really
depends on its mass.

The mass of a star determines
what's going to happen

after it finishes burning
its hydrogen fuel.

LEVIN:
All stars start out burning
hydrogen-- the lightest atom--

fusing hydrogen atoms
into helium,

working their way up
to heavier elements.

Gravity wants to crush
the entire mass of the star,

but the enormous energy released
by fusion pushes outward,

preventing the star
from collapsing.

IMARA:
Stars are stable because you
have an outward-moving pressure

due to nuclear fusion,

and that's balancing with
the inward force of gravity.

LEVIN:
Smaller stars can't fuse
elements heavier than helium.

But in the most massive stars,

fusion crushes heavier
and heavier atoms

all the way up to iron.

Iron is such a massive element,
it has so many protons in it,

that by the time you fuse iron,

you don't get
any energy back out.

LEVIN:
Iron is a dead end for stars.

Fusing atoms larger than iron

doesn't release enough energy
to support the star.

And without enough energy
from fusion

keeping the star inflated,

there's nothing
to fight gravity.

GLIKMAN:
And gravity wins.

And so the entire star
collapses.

LEVIN:
Very rapidly, trillions of tons
of material come crashing down,

hit the dense core,
and bounce back out,

blowing off the outer layers of
the star in a massive explosion:

(explosion roars)

a supernova.

The more mass, the more gravity.

So if the remaining core
is massive enough,

gravity becomes unstoppable.

TYSON:
There's no known force

to prevent the collapse
to an infinitesimally small dot.

(explosion roars)

LEVIN:
Gravity crushes
the stellar core down,

smaller and smaller and smaller,

until all its mass is compressed

in an infinitely small point:

a black hole.

The theory makes sense,

but most physicists remain
skeptical about black holes.

NATARAJAN:
Einstein and Eddington,
all the sort of, you know,

pre-eminent astrophysicists
in the 1930s through 1950s,

did not believe
that they were actually real.

It remained a solution,
a mathematical enigma,

for a very long time.

So it took a long time
for people

to even start looking for them.

LEVIN:
It's not until the 1960s
that the idea

of a supernova
creating a black hole

is taken seriously.

Princeton physicist
John Wheeler,

who had originally
been a skeptic,

begins to use a name
from history

for these invisible objects:

black hole.

The term "black hole"
actually originates in India.

The Black Hole was the name

of an infamous prison
in Calcutta.

LEVIN:
Still, no one has ever detected
any sign of a black hole.

Then, in 1967, graduate student
Jocelyn Bell

discovers a strange,
extremely tiny dead star

that gives off
very little light--

a neutron star.

The cold remains
of a stellar collapse,

the neutron star gives
astronomers more confidence

that black holes--
much heavier dead stars--

might also exist.

(explosion roars)

A half-century
after Karl Schwarzschild

mathematically showed
that black holes

were theoretically possible,

scientists have identified
a natural process

that might create them:
the death of large stars.

So these giant supernova
explosions

of extremely massive stars

make black holes.

NATARAJAN:
Any star that is born
with a mass

that's about ten times
the mass of the sun or higher,

will end in a black hole.

So our galaxy is replete
with little black holes,

which are the stellar corpses
of generations of stars

that have come and gone.

LEVIN:
So what are these invisible
stellar corpses like?

Imagine I'm exploring space

with some advanced technology
for interstellar travel,

so that we could visit
a black hole--

maybe one in
our own galactic neighborhood.

This particular black hole
isn't very big,

only about ten solar masses--

meaning ten times
the mass of the sun.

And like all black holes,
it has an event horizon--

a distinct edge to the darkness.

That's the boundary Karl
Schwarzschild first discovered,

where gravity is so strong
that nothing can escape--

not even light.

And that's where we're going.

(engine runs, machine chirps)

♪ ♪

♪ ♪

LEVIN:
As we get closer, some very
strange things begin to happen.

Look at the edge
of the black hole--

see how the image
of distant stars

is distorted and smeared
into a circle?

That's gravitational lensing.

The black hole's extreme gravity

bends the path
of light passing by,

so that a single point of light,
like a star,

briefly appears as a ring
around the event horizon.

♪ ♪

I'm now deep in
the black hole's gravity well,

and we're going to start
experiencing the effects.

The extreme gravity
actually slows down time

relative to the Earth.

From their point of view...

(audio slows):
I appear to be slowing down.

But from my point of view,
time on Earth is speeding up.

Now, let's say I want
to get even closer,

by taking a spacewalk.

♪ ♪

(machines beeping and hissing)

The way the black hole
slows down time

is about to get
even more pronounced.

To keep track of the changes
I'm about to experience,

I'm turning on
this strobe light.

It'll blink once a second.

From here, I can see the shadow
of the event horizon approaching

and my light blinking normally.

But watching from the ship,

the closer I move
toward the black hole,

the more slowly
I appear to move.

The pulses are
nearly infinitely spaced,

so it looks as though
I'm frozen in time.

For me, everything is
completely normal.

Even when I reach
the event horizon.

If you waited long enough--

maybe millions
or billions of years--

the ship would finally
see me disappear.

And that's the last
you'd see of me.

What's inside a black hole?

That's still a mystery.

And even if I find out, I can
never go back and tell you.

But I can say this: black holes
may be dark from the outside,

but inside, they can be bright.

I can watch the light
from the galaxy

that's fallen in behind me.

And that's the last thing
I'll ever see.

Unfortunately, the fun
is about to end.

♪ ♪

Now that I've crossed
the event horizon,

I'm falling toward the center,

where all of the mass of
the black hole is concentrated.

And I'm beginning to get
stretched.

As I fall in, the gravitational
pull at my feet

is stronger than at my head,

and my body is starting
to get pulled apart.

I'll be stretched as long
and thin as a noodle--

spaghettified.

And ultimately, I'll end up

completely disintegrating
into my fundamental particles,

which are then crushed
to an infinitely small point.

A singularity,
where everything we understand

about space and time
breaks down.

Or maybe the black hole--

less than 40 miles across
on the outside--

is as big as a universe
on the inside.

And as I pass through,

my particles will join
the primordial soup

of a new beginning.

So that's what theory tells us
we might experience

if we could travel
to a black hole.

♪ ♪

♪ ♪

But how can we know for sure?

How do you investigate something
you can't even see?

There are ways to investigate

if something
is happening somewhere,

even if I can't see that thing
directly.

Take Yankee Stadium:

what's happening inside there?

Is there a game going on?

I can't see the field.

I can't see any players,
or baseballs, or bats.

But I can definitely tell

if there's activity
around the park.

It's pretty clear
something is going on.

♪ ♪

It might seem obvious,
but whatever it is,

I can learn a lot just by
observing the happenings

around the stadium.

And these do look a lot
like baseball fans.

♪ ♪

(bat hits ball)

(crowd cheers, organ plays)

And that's the way
we investigate black holes:

by observing the effect
they have on their surroundings.

But what sort of effects?

How might a black hole
reveal itself?

Starting just before
World War II,

two monumental discoveries

are about
to radically change astronomy.

In 1931, Bell Labs
engineer Karl Jansky

picks up mysterious radio waves
emanating from deep space.

Then the sky
gets even stranger--

when scientists
mount Geiger counters

on captured German rockets

and discover the cosmos
is also full of X-rays.

These discoveries give
astronomers important new tools

that will revolutionize
the hunt for black holes

and dramatically
expand our vision.

(machine beeping)

BARTUSIAK:
What our eyes can perceive

is a very narrow part
of the electromagnetic spectrum.

LEVIN:
If the electromagnetic spectrum

were laid out
along the Brooklyn Bridge,

the portion we can see
with our eyes

would be just a few feet wide.

Electromagnetic radiation

includes waves of
many different frequencies:

radio waves, microwaves,
infrared and ultraviolet light,

X-rays, and gamma rays.

Radio and X-ray astronomy
open up the sky,

revealing dim or
even invisible objects

blasting out powerful energy
no one knew was there.

They began to realize

that this very placid thing
that we see out there,

all this very quiet thing that
looks like nothing is happening

and the only thing
that's moving is the planets,

found out that there
was madness going out there.

It was chaos out there!

LEVIN:
X-rays come from the
high-energy end of the spectrum.

What is creating
all this energy?

This much thing is certain:
whatever the source,

it is invisible
to ordinary telescopes.

And it is hot.

PAUL MURDIN:
X-rays come from things

which are at temperatures
of millions of degrees.

Even tens of millions.

LEVIN:
One of the first
of these X-ray sources

to catch the attention
of astronomers

is named Cygnus X-1.

Cygnus, it was
in the constellation Cygnus;

X, it was an x-ray source;

one, it was the first one
you found.

LEVIN:
In 1970, Paul Murdin
is a young English astronomer

trying to secure his next job.

MURDIN:
I was a research fellow,

I was coming to the end
of my three-year contract,

and I thought, "What can
I contribute to finding out

what these things are?"

♪ ♪

LEVIN:
Murdin works
in a 15th-century castle

surrounded by telescopes--

the Royal Observatory.

Using the largest telescope
in England,

he begins searching the area

of the constellation Cygnus,
the swan.

He decides to hunt
for pairs of stars.

Pairs of stars
are called binaries.

They may sound exotic, but
they're not at all uncommon.

Many of the stars we see--
perhaps half--

are actually binaries,

pairs of orbiting stars
locked together by gravity.

But Murdin wonders: Is it
possible there are binaries

where only one of
the stars is visible?

MURDIN:
I thought that maybe there was
a kind of a star system

in which there was a star, one
ordinary star that made light,

and then there was another star
nearby that made X-rays.

LEVIN:
The telltale sign of a binary

is that the stars are moving
around each other.

So Murdin begins searching
for a visible star

that shows signs of motion.

Sometimes it's coming towards
you, sometimes it's coming away.

Sometimes it's coming towards
you, sometimes it's coming away.

LEVIN:
When the star is moving toward
us, it appears more blue,

as the wavelength of its light
gets shorter.

Moving away,
it appears more red,

as the wavelength of its light
gets longer.

This is known as Doppler shift.

After looking for color changes

in hundreds of stars
in the area of Cygnus,

Murdin spots
a possible suspect--

a visible star whose light
is shifting,

as though moving around.

MURDIN:
It very clearly was
a binary star, a double star.

The star was moving around
and around with a period,

going around once,
every 5.6 days.

LEVIN:
But whatever it's going around
can't be seen.

MURDIN:
There was no trace in the
spectrum of the second star.

There was one star there.

There wasn't
the second star there.

LEVIN:
Murdin has a binary pair in
which only one star is visible.

The second object emits X-rays,

has enough mass and gravity
to dramatically move a star,

but gives off no light.

Could it be the corpse of a star

massive enough
to become a black hole?

KIP THORNE:
The crucial issue in deciding

whether Cygnus X-1
was a black hole

was to measure the mass
of the X-ray-emitting object.

LEVIN:
It would have to be
very massive,

at least three times
the mass of our sun.

If not, it's probably
just a neutron star--

a collapsed star that's dense,

but not heavy enough
to be a black hole.

THORNE:
So the observers needed
to come up with a conclusion

that the dark object,

the X-ray-emitting object
in Cygnus X-1,

was heavier, hopefully
substantially heavier,

than three solar masses.

LEVIN:
From his observations, Murdin
is able to make an estimate

of the mass
of the invisible partner.

And the answer came out to be
six times the mass of the sun.

So there was a story, then,

that Cygnus X-1
was a black hole.

And the key to the argument was

that the mass of the star
you couldn't see

was more
than three solar masses.

When I'd finished writing it all
out, I sat back and thought,

"It's a black hole."

♪ ♪

LEVIN:
This would be the first actual
detection of a black hole.

It's a huge claim, and Murdin
will have to convince skeptics,

starting with his boss.

MURDIN:
The Astronomer Royal,
Sir Richard Woolley.

He didn't really go
for black holes.

"It's all fanciful..."

It's kind of-- a lot of people
in California

were talking about this.

There are a lot of
funny people in California.

(chuckles):
You know, a lot
of hippie-type people.

LEVIN:
People like theorist Kip Thorne.

So I was nervous about it.

I was nervous about
the scale of the discovery.

And actually so were other
people all around me.

I was working with a fellow
scientist, Louise Webster.

And we were modest about the
claim that we were making

because we knew what
people would think of it.

And if you look
at the paper we published,

it just mentions the word "black
hole" once, right at the end.

"We think this might be
a black hole."

LEVIN:
The Paul Murdin-Louise Webster
paper appears in September 1971.

Other astronomers agree:
It could be a black hole.

But no one knows for sure.

Three years later,

Kip Thorne and the noted British
physicist Stephen Hawking

make a now-famous wager
about Cygnus X-1.

We made a bet
as to whether Cygnus X-1

really was a black hole or not.

LEVIN:
The bet is partly in jest.

Both men hope
it is a black hole.

But Hawking, not wanting to jinx
it, bets against his own wishes.

THORNE:
Stephen claims that Cygnus X-1
is not a black hole.

And I claim it is a black hole.

And so we signed that bet
in December 1974.

And gradually, the case
that it really was a black hole

became stronger and stronger
and stronger.

So in June of 1990,
Stephen broke into my office

and he thumb-printed off
on this bet,

conceded the bet in my absence.

I came back from Russia and
discovered that he had conceded.

LEVIN:
Now, by 1990, the evidence
of Cygnus X-1's mass

may be strg enough to settle
a bet between two friends.

But the original estimate wasn't
precise enough to be definitive.

In order to calculate mass,

Paul Murdin had
to rely on rough estimates

of the distance to Cygnus X-1,

which varied by a factor of ten.

And the question wouldn't be
answered for another 20 years,

until astronomer Mark Reid
became intrigued by the puzzle.

Reid is an astronomer

at the Harvard-Smithsonian
Center for Astrophysics

when he sets out
to conclusively prove

that Cygnus X-1 is a black hole

by measuring its precise mass.

But how can you measure the mass
of an invisible object?

Using laws developed

by German astronomer
Johannes Kepler

in the 1600s,

it's possible to calculate
the mass of a celestial object--

but only if you know
its distance.

REID:
Distance in astronomy
is absolutely fundamental.

If you don't know distance, you
don't know what the object is.

It could be a very nearby
firefly-like thing.

It could be a very distant,
huge star,

much, much bigger than the sun.

LEVIN:
So to get the true,
precise mass of Cygnus X-1--

and confirm
that it is a black hole--

Reid needs to know
how far away it is.

But how can he measure
the distance to a star?

The secret lies in a familiar
phenomenon: parallax.

It's what our eyes and brains
use to see in three dimensions.

You can put your finger up
at arm's length,

look at it,
and close one eye.

I'm closing my left eye.

And I'm looking at my finger

relative to the wall
in the background there.

And now if I open my eye,
close my right eye,

I see my finger
has appeared to move

with respect
to the original position.

And that's because
our eyes are separated,

and we view from
different vantage points.

LEVIN:
To use parallax

to measure distance
to an object in the sky,

astronomers let the motion
of the Earth

provide the two different
vantage points.

Imagine Cygnus X-1
is right here.

And the Earth and the sun
are over there.

Now, the Earth goes
around the sun once a year.

And in the springtime, the Earth
ends up on one side of the sun,

and we observe Cygnus X-1
along a ray path like this.

Then six months later,
the Earth goes around the sun

to the other side.

We get a different vantage point
from Cygnus X-1.

LEVIN:
Now he has a triangle that goes

between the Earth
at its two positions

and Cygnus X-1.

We know the base
of the triangle,

the diameter of Earth's orbit.

And the principles of geometry
tell us

that all we need
to calculate the distance

is the size of
the angle at the top.

And we measure
this very small angle here,

at the point at Cygnus X-1.

And then from direct geometry,

we can calculate the distance
to Cygnus X-1

and from that infer
a very accurate mass.

LEVIN:
The concept is simple.

But Cygnus X-1 is so far away

that the angle to be measured
is miniscule--

a tiny fraction of one degree.

It's smaller than the angle
spanned

by Abraham Lincoln's nose

on a penny in San Francisco
viewed from New York.

Because the angle
is so very tiny,

it can't be measured
by any one telescope.

But Reid's team has a solution.

We take ten radio telescopes

that are spread
across the continental U.S.

and to Hawaii and to St. Croix
in the Virgin Islands.

We use these telescopes
simultaneously,

and we synthesize in a computer

a telescope that has a diameter
of the size of the Earth.

That gives you incredible
angular resolution.

LEVIN:
Using this technique,
Reid's team determines

that Cygnus X-1 is
6,000 light years away.

REID:
With the new distance we got,
the 6,000-light-year distance,

we're able to determine
that the mass

is about 15 solar masses,

easily a black hole.

LEVIN:
40 years after it was identified
as a possibility,

Cygnus X-1 is
now widely accepted

as the first confirmed
black hole.

MURDIN:
It's an understated paper,

and the fact
that my name was on it

and Louise Webster's was on it,

did us a lot of good
in our careers.

I think as a result
of this discovery,

I got offered a permanent job.

And it was a great celebration
for the family.

So it worked out very well
for me--

as well as getting
the intellectual satisfaction

of solving a problem.

LEVIN:
So finally, after years
of speculation,

we have a real black hole.

Not only that, but a black hole
that's blasting out X-rays

and has a companion star.

If we could visit
in my imaginary spaceship,

what would we see?

The distance to Cygnus X-1

has been established
at 6,000 light years from Earth.

And its mass is 15 solar masses,
or 15 times the mass of the sun.

And Cygnus X-1 is surrounded
by an accretion disk--

a disk-shaped cloud of gas and
dust outside its event horizon,

the point of no return.

As gravity pulls matter
toward the black hole,

the cloud starts rotating,

just like water
being pulled down a drain.

Within that accretion disk,

particles closest
to the black hole whip around

at half the speed of light.

It's like a giant
particle accelerator in space.

But why does it emit X-rays?

As those particles race around,
they collide,

which heats them up
to millions of degrees.

When they get that hot,
particles blast out X-rays.

And it's those X-rays that
first led astronomer Paul Murdin

to investigate this black hole
nearly five decades ago.

♪ ♪

And there's something else
about Cygnus that's different:

It has a companion star.

This blue super-giant star

orbits the black hole
once every 5.6 days.

It orbits so close to Cygnus X-1

that the black hole
strips material off the star

and pulls it
into the accretion disk.

Some of that material
will cross the event horizon

and get swallowed up,
but not all of it.

OZEL:
Some of the stuff
actually comes back out

before ever entering
the black hole.

Kind of like a toddler eating:

Half the pasta ends up
on the floor,

half of it may be
on the ceiling,

and some of it in the mouth.

One of the most striking

and enigmatic features
of Cygnus X-1

is its enormous jets.

These beams of particles
and radiation stream outward

from Cygnus's
north and south poles,

perpendicular
to the accretion disk.

♪ ♪

There's still a lot
we don't know about these jets,

but they are tightly focused
and extremely powerful,

blasting out at nearly
the speed of light

and extending
well beyond Cygnus.

OZEL:
When gas gets
to these high temperatures

and produces the light,

there's also a little bit
of a magnetic field

that forms around them.

And we don't understand
exactly how,

but these magnetic fields

help collimate these massive
outflows from black holes,

powerful hoses if you will,
that just spew matter out.

LEVIN:
So that's Cygnus X-1,
if we could see it up close--

a growing, feeding black hole
with huge jets

blasting particles way out
into the universe.

NATARAJAN:
They're almost these breathing,

fire-eating demons, if you will.

They flicker, they have bursts;

it's a very violent fireball,
very active.

LEVIN:
What was once a bizarre
mathematical curiosity

has now become quite real.

(explosion roars)

After decades of skepticism,

scientists now accept
that burned-out corpses

of large stars

can trap light inside them,

warp space and time
around them,

attract matter, and accelerate
it to mind-boggling speeds.

GALISON:
Black holes seemed like
such a radical idea

that we shouldn't accept it.

But bit by bit, the evidence
for black holes

has gotten stronger
and stronger.

And we've seen
these amazing things.

♪ ♪

LEVIN:
At least 20 black holes
have been found in our galaxy,

X-ray binaries, like Cnus X-1.

And there are probably
millions more

of these massive stellar corpses

in our galaxy alone.

Still, a stunning
surprise awaits.

Everything astronomers think
they know about black holes--

and much of what they believe
about the universe itself--

will be upended
by a shocking discovery.

The revelations begin when radio
telescope surveys of the sky

detect mysterious hot spots
emitting radio energy.

(whirring)

They were coming
from what looked like stars.

LEVIN:
Because these objects
resemble stars,

but were discovered
through radio signals,

astronomers name them
quasi-stellar radio sources--

quasars.

But are they stars or not?

The first step
in investigating them

is to figure out
what they're made of.

To do that, astronomers analyze

the electromagnetic energy
they emit.

Every element has a unique
spectral fingerprint.

For example, carbon.

Helium.

Hydrogen.

These lines reveal
the chemical make-up of a star.

But the spectrum of a quasar

turns out to be
incomprehensible.

BARTUSIAK:
They looked at it
and it was gibberish.

It didn't look like
there were any emissions

from elements that they knew.

LEVIN:
What are they missing?

There has to be
a clue somewhere.

Finally, in 1963, Caltech
astronomer Maarten Schmidt

finds it hiding in plain sight.

Buried in the quasar's spectrum
is the fingerprint of hydrogen.

He noticed something familiar,
but it was in the wrong place.

The fingerprints of hydrogen had
been shifted way off to the red.

LEVIN:
It was hard to spot because
the spectral lines of hydrogen

were radically shifted toward
the lower-frequency end

of the spectrum.

And that could only
mean one thing.

♪ ♪

The quasar is moving away
from us at fantastic speed.

But astronomers have never
before seen light shifted

to such an extreme.

(barking, audio slowing down)

Like a familiar sound shifting
too low to understand,

the light from quasars
has shifted to such a degree

that hydrogen is unrecognizable.

This extreme amount of shift

means quasars are racing away
from us at blinding speeds.

The reason?

It's the legacy of an event

that occurred almost 14 billion
years ago: the Big Bang.

(explosion roars)

The beginning of our universe.

And ever since, the universe
has been expanding,

carrying with it all the objects
it contains, including quasars.

GLIKMAN:
No one had ever seen anything
moving away at that high speed.

This made this object
the furthest-away thing

that had ever been seen,

which meant the thing itself
had to be so luminous,

and you had to account for that.

BARTUSIAK:
Two billion light years away,
putting out the energy

of a trillion suns each second.

What could possibly create that?

No one had any idea what could
be powering these things.

Where could all
of this energy come from?

If you work out
through calculations,

it can't be chemical energy.

(explosion roars)

They knew it couldn't
be nuclear energy.

(explosion roars)

LEVIN:
There's no way a quasar
could be a star.

No amount of nuclear fusion

could produce
that much star power.

The only engine
that could possibly

put out that much energy
is gravity.

LEVIN:
Gravity.

In everyday life, we can
overcome gravity easily.

But when concentrated
to an extreme by a black hole,

gravity is
overwhelmingly powerful.

A handful of scientists
start wondering:

Could quasars perhaps
be powered by gravity engines?

What if the energy blasting out
from quasars

is coming from bright accretion
disks around black holes?

NATARAJAN:
To produce that kind of energy,

that kind of brightness,

it has to involve a black hole.

LEVIN:
But not just any black hole.

THORNE:
Whatever was the source
of the emission from a quasar

had to be massive.

How massive?

Well, millions or billions
of times heavier than the sun.

LEVIN:
Millions or billions of times
heavier than the sun.

Cygnus X-1 is only 15 times
the mass of the sun.

The black holes powering quasars

are an entirely different
category of black hole:

supermassives.

♪ ♪

And they seem to be located
in the centers of galaxies.

But what about our own galaxy?

Could there be any supermassive
black holes closer to home?

The center, where any
supermassive would be found,

lies in the direction of the
constellation Sagittarius,

the Archer.

Now, Sagittarius
isn't just any constellation.

It's in the direction
of the center

of our own Milky Way Galaxy.

But since we live
inside the Milky Way,

we can't see the galaxy
the way a space traveler would.

But I can use my trusted
imaginary star machine

to show us the galaxy
from the outside.

Our home is a spiral galaxy,
hundreds of billions of stars,

drawn together
into a gigantic disk.

It's wide, about
100,000 light years across.

But it's relatively thin,

only about
1,000 light years thick.

And the whole spiral
slowly rotates.

Our solar system is here.

And here, 26,000 light years
from the Earth,

is the center, which we see
in the direction of Sagittarius.

In this dense center,
there are millions of stars,

and lots and lots
of dust and gas.

So that's the view of our galaxy
from the outside,

thanks to
my imaginary technology.

But since we live
inside the Milky Way,

when we look towards the center,

we're looking through much
of our own galaxy,

which means it appears to us

as a band of stars and dust
across the sky-- a milky way.

♪ ♪

Deep inside this band
of stars and dust,

could a supermassive
black hole be lurking?

GHEZ:
The data that
we're getting now...

LEVIN:
In the 1990s, astronomers grow
determined to solve the mystery,

to peer through
the murky Milky Way

and learn what, if anything,
is at its center.

One of them is Andrea Ghez.

GHEZ:
One in 20...

LEVIN:
Ghez takes on
a daunting challenge.

She will try to track
individual stars

orbiting the center
of the galaxy.

GHEZ:
The essence of this experiment
comes from watching

stars orbit the center
of the galaxy.

So you want to find the stars

that are as close to the center
of the galaxy as possible.

Which means that
I want to get access

to the largest telescope
I can possibly get my hands on.

LEVIN:
And that means coming... here.

♪ ♪

The summit of Mauna Kea,
a dormant volcano

almost 14,000 feet
above the beaches of Hawaii.

High altitude and low humidity

make this the ideal place
for astronomy.

♪ ♪

The instrument Ghez uses
is Mauna Kea's Keck Observatory,

one of the largest in the world.

But despite its size,
Keck has the same problem

as all telescopes on Earth:

atmospheric distortion.

GHEZ:
Think about looking at a pebble

at the bottom of a river.

The river is moving very quickly

and your view of that pebble
is distorted.

LEVIN:
Like a river,

the Earth's atmosphere
is constantly changing,

bending light
like a funhouse mirror.

To compensate for this,
Keck pioneers the scientific use

of a declassified
military technology

called adaptive optics.

First, they shine a laser
into the sky,

creating an artificial
guide star.

The turbulent atmosphere
distorts the guide star,

but the computer knows
what it should look like,

and adjusts the telescope mirror
accordingly.

GHEZ:
So if you look at yourself
in a circus funhouse mirror,

you look completely distorted.

And the goal
of the adaptive optics system

is to introduce a second mirror
that's the exact opposite shape

and make you look flat again.

LEVIN:
Buried deep inside
the telescope,

the deformable mirror
changes shape

up to 2,000 times a second

to reverse the atmosphere's
distortion.

GHEZ:
And it has allowed us
to take the sharpest images

ever obtained
of the center of the galaxy.

LEVIN:
The sharpness of those images
allows Ghez

to make out individual stars
near the center--

a huge advance in astronomy.

She begins recording
their positions in 1995.

GHEZ:
And every year since then,

we've taken an image--
just take a picture.

LEVIN:
Putting those annual snapshots
together

creates a time-lapse movie
of stellar orbits.

And what those movies reveal
is astounding.

♪ ♪

The stars are whipping around
the center of the Milky Way

at phenomenal speeds.

These things are moving
at several thousand,

up to 10,000 kilometers,
per second,

or ten million miles per hour.

They're, they're really hauling.

LEVIN:
To go that fast,
the stars must be orbiting

something extremely massive.

GHEZ:
The mass that we infer

is four million times
the mass of the sun.

What could be four million times
the mass of the sun

yet be completely invisible?

That is the proof
of a black hole.

LEVIN:
And not just any black hole--

a supermassive,
silent and sleeping,

right in the center
of our own galaxy.

In fact, this is
the best evidence to date

that we have for the existence
of supermassive black holes,

not only
in the center of our own galaxy,

but anywhere in the universe.

♪ ♪

A supermassive black hole

four million times
the mass of the sun,

in the very center
of our own Milky Way galaxy.

From a cosmic perspective,
it's right next door.

And it raises
a profound question.

There are billions of galaxies
out there.

If ours has a supermassive
black hole at its center,

and if quasars are found
at the centers

of their galaxies,

what about the others?

♪ ♪

Are there black holes
at the centers of galaxies?

If they are,
how common are they?

We simply didn't know.

LEVIN:
Could astronomers ever hope
to find what lurks

at the centers
of other galaxies,

millions of light years away,
as Ghez did in our Milky Way?

(engine ignites loudly)

It would take another innovation
in astronomy

to make that possible.

ANNOUNCER:
And lift-off of the space
shuttle Discovery,

with the Hubble Space Telescope,
our window on the universe.

LEVIN:
When the Hubble Space Telescope
starts delivering clear images

of distant galaxies,

a team of astronomers
gets to work.

They become known
as "the Nukers"

because their focus
is galactic nuclei,

the centers of galaxies.

One of them is Tod Lauer.

Step one,
we take a picture of the galaxy

with the Hubble Space Telescope.

It shows us where the stars
in the galaxy are.

It tells us its structure
in exquisite resolution.

♪ ♪

LEVIN:
The key to finding
supermassive black holes

is to learn how fast the stars
in the galaxy are moving.

Galaxies outside our own
are much too far away

to measure the speed
of individual stars.

But by analyzing the way light
is shifted from blue to red

at different points
in the galaxy,

astronomers can put together
an average speed of stars

orbiting the center.

It's accurate enough to create
a replica in a computer.

The second step,
where the real work begins,

is to try to model
the observations.

And we actually do that
by building models of galaxies

in the computer.

LEVIN:
It's known as
Schwarzschild's method,

developed by Princeton
astronomer Martin Schwarzschild,

son of Karl Schwarzschild,

whose mathematics
first described

the possibility of black holes.

LAUER:
Martin Schwarzschild's trick
was,

he would actually build up
a model of the galaxy

that not only had
where the mass was,

but it also had
how the stars were moving.

♪ ♪

LEVIN:
For each galaxy
they investigate,

the Nukers painstakingly build
a computer model and then,

using trial and error,

adjust the parameters
of mass and velocity--

trying to make the model
match the original observations

they got from the Hubble.

LAUER:
And we say,
"Let's try a star here,

"let's try one over here.

"Let's have it go around
this way.

Let's have this one go around
that way."

And we do this thousands
and thousands of times

until we build up a library

of how stars can orbit
in this galaxy.

Success is when observations
of the model

match the observations taken
with the Hubble Space Telescope.

LEVIN:
But that doesn't happen.

The models are missing
something.

We try it again and again
and again,

all with no black hole yet,
and we say,

"Gee, we really can't get
the observations explained

by the model."

LEVIN:
Only when they add
an enormous invisible mass

at the galaxy's center

does the model match
the Hubble observations.

LAUER:
Almost always
we have to put in

a black hole at the center.

We can't match the observations

without a black hole
in the model.

♪ ♪

LEVIN:
Of roughly three dozen galaxies
that the Nukers investigate,

virtually all of them require
a supermassive black hole.

And since then,
other observations have made us

even more certain

that supermassives and galaxies
go together.

Every galaxy
we've looked for one,

we have found a supermassive
black hole in its center.

LEVIN:
It's a stunning revelation.

Supermassives--

once an entirely unexpected
category of black holes--

may be common,

not only at the center
of our galaxy,

but of all galaxies.

Take galaxy M31,

also known as
the Great Andromeda Galaxy.

It's two-and-a-half million
light years away.

On a clear night,
you can see it from Earth.

But even with
the Hubble Space Telescope,

we can't make out
precise details of its center.

Still, we're pretty sure

there's something extremely
massive hiding there.

♪ ♪

What if we could take
a closer look?

What if we could visit
a galaxy far, far away?

♪ ♪

As we enter the outer part
of Andromeda,

we're still too far away to see
what's lurking at the center.

But we can make out

a dense cluster of stars
in the core,

and that could be a sign

that there's a giant black hole
nearby.

♪ ♪

Billions of years ago,
it would have been surrounded

by gas and stars
and other small black holes.

The black hole
may have powered a quasar,

feeding mad, and blasting out
blinding radiation.

Over hundreds of millions
of years,

it would have consumed

all the available gas
and the closest stars.

♪ ♪

(screen beeping)

♪ ♪

These days
it's relatively quiet.

But it has some
distinctive features

we've never seen before.

First, it's colossal.

If it were dropped
in our solar system,

Mercury, Venus, Earth, and Mars

would all be trapped inside
the event horizon.

That's big, but it's nothing
compared to the sheer mass:

100 million times
the mass of the sun.

And the destruction
won't end there.

Jupiter won't last long.

The gravitational field
of the supermassive

will grab hold
and swallow it whole.

Eventually, Saturn will suffer
the same fate.

The outer planets might survive,
but in cold and dark orbits.

♪ ♪

This black hole rotates rapidly,

distorting and dragging
the fabric of space-time.

Like all black holes,

the event horizon
is completely featureless.

Remember, there's nothing there.

It's just a boundary
that conceals the interior.

But the accretion disk
can tell us a lot

about what's going on.

That's the fiery ring of gas
and dust around the black hole.

♪ ♪

Imagine if we could release
a swarm of autonomous robots

to explore the accretion disk.

♪ ♪

The disk is spinning
at an incredible speed--

as much as half the speed
of light.

If Jupiter moved that fast,

it would complete
its entire orbit in a few hours.

The region around the black hole
is a cosmic tornado.

Now our swarm is caught
in the whirlwind, too.

They're like tracers
dropped into the storm

to map the movement.

The middle robot
can send us images.

It's following the leader
like a race car

speeding around the track.

From here, the extreme warping
of space-time

around the black hole

plays crazy tricks on our eyes.

It looks like
there's one accretion disk

whipping around the equator,

and another arcing
over and under the poles.

But that's an illusion.

The black hole's extreme gravity
bends the path of light

emitted behind the black hole,

and makes it look
like the accretion disk

is both above and below.

There's actually nothing
around the poles.

It's just the passing
light rays.

That's gravitational lensing
again.

Drawing much closer
to the event horizon,

the gravitational lensing
would become so extreme

that one of my robots could look
straight ahead

and eventually see its own back,

the light forever trapped
in an eternal circle.

So that's our tour
of the supermassive black hole

at the center
of the Andromeda Galaxy.

Pretty amazing.

Also amazing:
nothing in the mathematics

led scientists to imagine that
black holes could get that big.

♪ ♪

As strange as they are,

ordinary stellar-mass
black holes

were at least predicted
by theory.

Supermassives
are a complete surprise.

♪ ♪

For the stellar-mass
black holes,

people thought about them
from a theoretical perspective.

And then we found them
observationally.

The supermassive black holes,
the story has been inverted.

We actually found evidence
of them observationally first.

And now we're working
on the theory

of, how did these things
come into being?

♪ ♪

LEVIN:
We already know
that stars can collapse

to create ordinary black holes.

But supermassives are bigger
by many orders of magnitude.

Cygnus X-1 is 15 times
as big as our sun.

The supermassive
at the center of our Milky Way

is four million times
as big as our sun.

The one in the Andromeda galaxy

is 100 million times
as big as our sun.

And it's not the biggest--
not even close.

There are supermassives
ten, even 20 billion times

the mass of our sun.

How is it possible to make
such gigantic black holes?

Could supermassives
have come from collapsed stars?

That seems very unlikely--
we don't know any stars

billions of times bigger
than the sun.

TYSON:
We know about black holes
you might get from a dying star.

They have several times
the mass of the sun

contained within them.

But millions of times
the mass of the sun.

If that's the case, a dying star
cannot have possibly made it.

LEVIN:
So do these supermassives--

millions or even billions
of times heavier than the sun--

somehow just grow, packing it on
like voracious giants?

The wild thing about black holes
is that they feed.

They're constantly devouring
anything that comes

within their sphere
of influence,

so they grow.

LEVIN:
But how exactly do they grow?

What do they eat,
and where do they find it?

NATARAJAN:
We believe that black holes grow

by accretion of gas.

And the way this works is that
you have a lot of gas around

in the center of a galaxy,

and this gas would then assemble
and form an accretion disk.

LEVIN:
The accretion disk
is made up of hydrogen, helium,

and other elements
in a gaseous form.

The immense gravity
of the black hole

pulls the gas in toward it.

As it swirls around,

it orbits closer and closer
to the black hole,

and the feeding begins.

NATARAJAN:
The stuff in the inner regions
would get slowly pulled in,

sped up,
will reach the event horizon,

and then that's it.

LEVIN:
Whatever gas crosses the event
horizon disappears forever.

The black hole
has absorbed that material.

So it actually adds
to the mass of the black hole.

LEVIN:
So this is one way
a black hole can grow:

gradually nibbling gas and dust.

But it's not the only way.

Cygnus X-1 has been
slowly stripping material

off a nearby star--

a process that will likely go on

for thousands or millions
of years.

But what if a black hole
could rip an entire star apart

in just a matter of years,
or even weeks?

That would be
a very violent event.

And a team of space explorers
is on the lookout.

This is the Operations Control
Center for a space telescope...

I have you five-by-five...

We show beginning of track
at 0330.

LEVIN:
...the Chandra X-Ray
Observatory.

(people talking on radio)

LEVIN:
Orbiting up to 86,000 miles
above the Earth,

Chandra takes
high-resolution images

of objects that emit X-rays.

This is one: a short-lived,
extremely violent event

called a transient,

which fascinates
James Guillochon.

GUILLOCHON:
Supernovae, the destruction
of planets by their host stars.

Yeah, I'm just fascinated with
destroying things for science.

LEVIN:
James is investigating a mystery
discovered by a colleague,

Dacheng Lin.

This blur on James's screen

is actually a massive sudden
burst of X-ray energy,

caught by accident.

GUILLOCHON:
This little smudge popped up
in the background of this image.

And given its great distance,

it's actually
tremendously bright.

LEVIN:
Could it be a black hole
caught in the act of being born

in the violent collapse
of a huge star, a supernova?

(explosion roars)

Perhaps.

But the intense radiation
released by supernova

would only linger
for a few months.

♪ ♪

So how long has this mystery
object been blasting out X-rays?

To find out, they look at images
of that same part of the sky

taken at earlier dates.

2015.

2011.

2008.

2005, July.

2005, April.

No X-rays detected.

But the X-rays are there just
three months later, in July.

And the powerful, bright signal
has continued

for more than ten years,

from July 2005 to the present,

far too long to be a supernova.

So what could it be?

A black hole that's not feeding
is quiet and completely dark.

It won't show up
on any telescope.

But a black hole that is feeding
is different.

When it feeds,
it blasts out X-rays.

So could this be a black hole

that's suddenly begun devouring
something big?

TYSON:
What effect will this have
on anything that comes near?

What would it do to a star
that wanders too close?

Well, it will flay a star
layer by layer,

ultimately devouring

the entire star.

♪ ♪

LEVIN:
Unlike Cygnus X-1,
this is no mere nibbling.

This is a ten-year
feeding frenzy,

a massive black hole devouring
an entire star

in a cosmic blink of an eye.

It's the result
of a chance collision--

when an unlucky star
wanders too close,

and the black hole's extreme
gravity actually rips it apart.

GUILLOCHON:
The gravity from the black hole

will progressively get stronger
and stronger

as the star gets near.

And at that point, the star
will begin to deform.

LEVIN:
It's called tidal disruption.

It's similar to the way
our moon's gravity

easily moves
all the world's oceans.

The tides caused by a black hole

would be billions of times
stronger

and much more violent.

where a star could be
ripped apart by the black hole.

So you would see sort of
a plume of light

from the last gasp
of the material in the star.

LEVIN:
But there is a chance for some
part of the star to escape,

as James illustrates.

As the star is elongated by
the black hole's tidal forces,

it will essentially be feeding
the black hole

at the same time as half of it
is trying to escape.

So everything above this point,
approximately,

will have the chance
of leaving the galaxy.

It's moving that rapidly.

And everything below this point

will fall back
onto the black hole

and eventually
be consumed by it.

LEVIN:
So this is another way
for a black hole to gain weight.

Unlike the slow steady nibbling
of Cygnus X-1,

this black hole is devouring
most of an entire star

in one gulp.

But whether a black hole
feeds suddenly,

by swallowing half a star,

or steadily, through accretion,

astronomers still face a problem
when they try to understand

how supermassives got so big--

the timing problem.

The trouble begins with
the very oldest supermassives:

quasars, those very bright,
very distant,

and ancient objects

first discovered
in the early 1960s.

The conundrum was when we
started finding these quasars,

very bright quasars,
very early on in the universe.

DALE KOCEVSKI:
They're giving off
so much energy

that they have to have very
massive supermassive black holes

at their center.

LEVIN:
But quasars are extremely
far away,

which means that they're part
of the very early universe,

which began
nearly 14 billion years ago.

NATARAJAN:
Bright quasars,

600 million years
after the Big Bang.

A fraction of today's age.

LEVIN:
And, they're enormous.

NATARAJAN:
So billion-solar-mass
black holes, these behemoths,

had to be in place
when the universe

was about 550 million years old.

Now you have a problem.

Because you have to grow
something really big,

really fast.

And you are bumping up against
sort of physical limits.

♪ ♪

LEVIN:
Whether a black hole
is nibbling

or gulping down its meal,

it turns out that accretion--
how black holes feed--

has a speed limit.

Named after English astronomer
Arthur Eddington,

the Eddington Limit
will not allow a black hole

to feed too fast

because of the light
blasting out

from its own accretion disk.

♪ ♪

GLIKMAN:
Light has a pressure.

So photons can impart
a force on something.

We see this in winds from stars:
Light is pushing out gas.

So there's a limit to how fast
you can feed a black hole

before its own luminosity
quenches its own growth.

LEVIN:
So given this speed limit,
how did early supermassives--

quasars--
get so big, so fast?

Could there be a way to bypass
the speed limit entirely?

NATARAJAN:
The problem is still
time itself.

How do you grow them

to a billion times
the mass of the sun?

What are the conditions that you
need for that kind of growth?

LEVIN:
Some scientists are now asking:
What if there's a way

to create a black hole

that's already much more massive
from birth,

giving it a head start?

NATARAJAN:
If there was
a physical mechanism

that would allow you to make
a black hole seed

which was much more massive
from the get-go,

then the timing crunch
is not as much of an issue,

and the growing problem
is not as acute.

LEVIN:
The answer, some believe,

is to create a black hole
directly from a cloud of gas:

a scenario called
direct collapse.

It starts with gas clouds
made of hydrogen, helium,

and other elements--

the same raw materials
from which stars are born.

The denser clouds
will start to collapse

under their own gravity.

And as they collapse,
parts that are more dense

will collapse more quickly.

And so what happens is,
the cloud fragments.

LEVIN:
Those fragments
continue collapsing

until the hydrogen atoms
within them begin to merge.

Nuclear fusion begins,
and stars are created.

But what if a giant gas cloud
collapsed without making stars?

We realized that there are
a set of physical conditions

that would allow you
to form a very large gas disk

prior to the formation
of any stars.

So this gas disk
starts getting unstable.

That would allow the mass
to sort of flow into the center

very, very rapidly

and make
a very massive black hole.

♪ ♪

LEVIN:
It's something we've all seen
in nature,

from tornadoes to bathtubs--

a vortex.

But on a supermassive scale.

If you're in a bathtub
and you pull the plug out

and you see the water flowing
in a vortex,

very fast down to the center,

that's exactly what happens.

LEVIN:
Direct collapse might be a way

to create very large black holes
early in the universe

from enormous gas clouds,

completely skipping
the star stage.

Because they would be
so large already at birth,

these direct-collapse
black holes

would have a head start,
helping them to quickly grow

into the enormous young
supermassives we see

in the distant universe.

NATARAJAN:
You could potentially have these
direct-collapse black holes.

So black holes
whose original masses,

seed masses,
the initial masses,

are about 10,000
to maybe 100,000 times

the mass of the sun,

and that they form
from the get-go with that mass.

♪ ♪

LEVIN:
Direct collapse may explain
how enormous early supermassives

got their start.

But there's another fundamental
question about supermassives.

What is their role
in the universe?

Is their existence
just a matter of chance?

Or are they connected
in some larger way

to the very structure
of the cosmos?

Supermassive black holes
don't exist in isolation.

They seem to live in partnership
with galaxies.

♪ ♪

Collections of millions,
billions,

or even trillions of stars
bound together by gravity,

galaxies are the fundamental
building blocks of our universe.

So are the supermassive
black holes at their centers

somehow fundamental
to their very existence?

TYSON:
We now just assume every galaxy,

even ones we have yet
to confirm,

will have a supermassive
black hole in their center.

KOCEVSKI:
It could be that instead
of simply being oddities,

that they are a key component
to galaxies,

a key component to the universe.

We've come in a very short time
to realize

that they likely inhabit
the centers of all the galaxies.

And that can really only happen

if there's some
symbiotic relationship

between the evolution
of a galaxy

and the supermassive black hole
in its core.

LEVIN:
What could that relationship be?

One intriguing clue
relates to size.

CHUNG-PEI MA:
The bigger the galaxy is,

the more massive the black hole
appears to be.

So these black holes
at the center

seem to know about
their larger-scale environment.

LEVIN:
So which comes first,

the galaxy or the supermassive
black hole?

It's not that simple.

It appears they somehow
grow in tandem.

GHEZ:
It's hard for one to form first
and affect the other.

So today we think
that whatever formed one

had to form the other
as a by-product of that process.

And that there has to be
some feedback mechanism

between the black hole
and the galaxy

that keeps the growth of the two
in lock sync.

♪ ♪

LEVIN:
The way galaxies grow
is by forming new stars

from clouds of hydrogen gas.

Gas is essentially
the fuel for star formation,

just like gas is the fuel
for our cars.

And so if you run out of gas,
you run out of new stars.

LEVIN:
So are supermassive black holes

somehow interfering
with star formation?

GLIKMAN:
When a black hole is growing,

a tremendous amount of energy
is being liberated

and sent out into the galaxy.

And so we think that some of
that energy goes to warm up gas.

And gas that's too warm will not
form stars anymore.

♪ ♪

LEVIN:
The heat produced
by a growing black hole

makes it impossible
for stars to form nearby.

♪ ♪

GLIKMAN:
And so one way
that a growing black hole

can influence its host galaxy

is by quenching
the star formation.

LEVIN:
In effect,
the growth of the supermassive

determines whether or not its
host galaxy grows or stagnates.

GALISON:
They have a kind of
eating phase,

and then a quiescent phase.

So they seem to be involved

with the formation of the galaxy
in that way,

and then stabilizing
of the galaxy at the same time.

LEVIN:
So these mysterious
supermassives

may actually control
the building of the universe--

not so much by their size,

but by the way the energy
they generate shapes galaxies.

By mass, if you count up all
the black holes in the universe,

the tiny ones as well
as the supermassive ones,

the ultra-massive ones,

black holes are nothing.

However, energetically,
how much power the galaxy gets

and at what time
as it assembles,

seems to be dictated
by the central black hole.

So they might well be
the key players in the universe.

♪ ♪

LEVIN:
In the next two years,
NASA plans to launch

the James Webb Space Telescope.

Humanity's most powerful
telescope ever,

the James Webb is designed
to look in the infrared,

allowing it to see farther
back in time than Hubble,

getting a look
at the first stars and galaxies

that formed after the Big Bang.

Hopes are high that
the James Webb Space Telescope

will help solve
many of the remaining mysteries

about the earliest
supermassive black holes.

TYSON:
The James Webb Space Telescope
is tuned specifically

to observe the early universe
when galaxies were being born.

That could give us
deeper understanding

of how you end up
with a supermassive black hole

in your galaxy
to begin with.

GHEZ:
Technology is moving
really fast,

and as a result, we have
really fundamental new views

of the universe.

I think we are really living
in a golden era of astronomy.

♪ ♪

LEVIN:
And the James Webb
Space Telescope

isn't the only new development
that promises to solve

some of the mysteries
around black holes.

♪ ♪

WOMAN:
I believe have
infrared components...

LEVIN:
A group of scientists

led by Shep Doeleman

is now attempting
the impossible:

to take a picture
of a black hole.

DOELEMAN:
It's interesting
that we can say something

about the accretion flow
near the black hole at all.

OZEL:
And if some of this
linear behavior survives,

maybe we'll have a way
of interpreting it.

LEVIN:
The project is called
the Event Horizon Telescope.

DOELEMAN:
The basic goal
of the Event Horizon Telescope

is really to see the unseeable.

It's to bring into focus

something that science
has told us for many, many years

is precisely something
we can't observe--

the black hole.

LEVIN:
Their primary target
is Sagittarius A ,

the supermassive in the center
of our Milky Way Galaxy.

They're using a global network
of radio telescopes.

DOELEMAN:
We need good weather
at eight different telescopes

all around the world,

and that is a tall order.

LEVIN:
But if black holes
are invisible,

what exactly do they hope
to photograph?

What we are trying to photograph
really is the shadow.

So as this gas
around the black hole

swirls inwards and actually hits
the event horizon,

it leaves a silhouette,

a very well defined shadow
on the surrounding light.

So really it should look
like a donut,

with its very well defined hole.

And that's the picture
that we're after.

If I convert that
into frequencies,

I get two-pi-square there.

LEVIN:
The team has conducted
their first observing run

and is processing the data now.

Okay, you're saying
the velocity...

LEVIN:
It's hoped that
these new technologies

will give us an unprecedented
view of black holes

in our universe.

But there is one new technology

that is already delivering
results.

And that brings us back here,
to LIGO,

a key player
in the black hole drama,

to an idea that took root
way ahead of its time:

gravitational waves.

With general relativity,
his theory of gravity,

Einstein predicts
that when an object moves,

it can create ripples
in space and time--

an actual squeezing
and stretching of space itself.

One of the holy grails
of 20th-century physics

was to detect
these gravitational waves.

WEISS:
That was not easy to do

with general relativity,

because all the effects
that you could think of

were infinitesimally small.

Very, very difficult to measure.

LEVIN:
The thinking was,

if gravitational waves
could be measured,

it would confirm
Einstein's prediction.

And there could be
an added benefit--

it might also prove
the existence of black holes

and help solve the mystery
of how supermassives grow.

But how to detect
gravitational waves?

In 1970,
the problem caught the attention

of a young experimental
physicist, Rai Weiss.

(classical music playing)

Rai had the perfect background
to hunt for gravitational waves.

For decades, he'd been working
with more familiar waves--

sound waves.

WEISS:
We were immigrants,

we were German Jews.

And a lot of our friends were
very, very interested in music.

(music continues)

LEVIN:
Rai devoted himself

to coaxing every subtle nuance
he could

out of recorded music.

WEISS:
Those records
had a terrible problem.

When the music was loud,
it sounded wonderful.

When the music
was real quiet and slow,

what you heard was this...

(imitating hissing)
...like that.

A hissing noise.

And that was so annoying.

LEVIN:
The lessons he learns

trying to eliminate noise
in recordings

will pay off later,

when Rai turns his attention

to detecting
gravitational waves.

WEISS:
You have to understand

how a gravitational wave
does its dirty work.

LEVIN:
As a physics problem,

gravitational waves
are not unlike sound waves.

Let's suppose the wave
comes from something

that is in some way
moving and oscillating.

(vibrating)

LEVIN:
A sound wave compresses
and expands air.

A gravitational wave
compresses and expands space

and everything in it.

WEISS:
If a wave came
through the Earth,

it would cause space

to expand momentarily
and then contract again.

It keeps doing it,
so it's this thing

that goes blip, blip, blip,
right along like that.

LEVIN:
So how to measure

the extremely tiny expansion
and contraction of space?

Rai's idea was to use light.

Send a beam of light

from one place to another,

and measure the time it takes
to get there.

(clicks)

That's how the exact distance
to the moon was calculated:

bouncing a laser beam
from the Earth

off a mirror left behind
by Apollo 11 astronauts.

♪ ♪

From the duration
of the round trip,

scientists could determine
the distance.

♪ ♪

Rai came up
with an ingenious design

for an instrument
that uses lasers and mirrors

to detect the faint expansions
and contractions of space

that would be caused
by a gravitational wave.

It's called
a laser interferometer.

It works by firing a laser
into a splitter.

Half of the light
continues straight ahead

towards one mirror,

while the other half
is sent towards another mirror.

The distant mirrors bounce
the light beams back,

where they rejoin
at a photo detector.

If the distances the two beams
travel are exactly the same,

the system is designed so the
two beams cancel each other out;

the detector sees nothing.

You've set the trap to measure
the gravitational wave.

Now comes the gravitational wave
that's coming,

let's say, at this structure.

LEVIN:
If a gravitational wave
passes through,

it briefly changes
the length of the arms.

The light beams no longer
arrive back at the same time

to cancel each other out.

A gravitational wave hits.

Light appears at the detector.

The trap has sprung.

That's the basic idea.

It's a very straightforward
measurement.

LEVIN:
A clever idea,
and simple in principle.

But the devil--

and the Nobel Prize--

lie in the details.

The difference in length
between the two arms

would be tiny beyond imagining.

How tiny?

Well, take the size of an atom.

It's less than that.

Go down by a factor of 100,000.

That's the nucleus of an atom.

It's less than that.

It was 100 times below that.

So we're talking about
really itsy-bitsy, teeny-weeny.

I thought it was crazy.

I think everybody's
initial reaction to the idea

was, this is going to be
impossible.

LEVIN:
In 1973, Kip Thorne puts
his skepticism on the record

in a classic textbook,

doubting it will ever work.

But Kip has never heard
Rai Weiss

explain his plan in detail.

And when he does...

We spent the whole night
talking.

And so I said, "No, no, no,
it's very possible."

And within no time at all,
20 minutes, maybe half an hour,

Kip was solidly understanding
this thing and he says, "Yup!"

And I ate crow
the rest of my career,

because once I had talked
with Ray about it in detail,

I decided I would spend
a large fraction

of the rest of my career

helping the experimenters.

LEVIN:
But it will take 40 years,

and enormous sums of money,

to bring Rai and Kip's vision
to reality.

Getting LIGO funded

was extremely controversial.

Hundreds of millions of dollars

to detect a signal
that had never been seen before.

There were many people
who feared

that LIGO would suck the money
out of the room.

And so there was
a lot of controversy.

What everybody could agree on
was,

this was extremely difficult.

LEVIN:
With such a sensitive
instrument,

one of the biggest challenges

is Rai Weiss's old
hi-fi nemesis: noise.

Ground motion.

The seismic motion of the Earth.

Acoustics' noise,

sounds...
(thunder crashing)

Everything would tend to move
that mirror.

LEVIN:
Turns out, even the emptiness
of a total vacuum

creates a potentially crippling
problem.

At subatomic distances,

the weird randomness
of the quantum world

causes a ruckus in the mirrors.

THORNE:
This quantum noise is due
to quantum fluctuations.

These mirrors are doing what
an electron does inside an atom;

they're jiggling around.

♪ ♪

LEVIN:
Exquisite sensitivity,

extreme vacuum,

hundreds of thousands
of electronic circuits...

LIGO is one of
the most complex instruments

in the history of science.

And as a final means
of eliminating false signals,

they build not one,

but two complete installations:

one in Washington state
and another in Louisiana.

And so the LIGO designers
did it right.

They designed
more than one detector,

separated from one another
by great distances,

so that if you detect something
in one and not in the other,

then, you know, go back
and check your electronics.

Check to see
if it was April Fools' Day

and somebody didn't just
tweak the knobs.

♪ ♪

LEVIN:
Early fall 2015.

Both locations are operating,

but the first official science
run has not yet begun.

They're still testing.

In the early hours
of Sunday, September 14, 2015,

a scientist in Louisiana
makes a fateful decision.

♪ ♪

Robert Schofield
has been working all weekend

doing final calibrations.

All righty,
let's take a spectrum.

LEVIN:
He has one last test.

SCHOFIELD:
So let's see where this
computer's getting its power.

LEVIN:
But it's late, and the equipment
is not cooperating.

SCHOFIELD:
It was about 4:00 or so
in the morning,

and we still had about
another hour of work to do.

And we were, like, "Yeah,
things aren't working so well,

"and I'm really tired.

Let's not do this last hour
or so of work."

LEVIN:
They call it a night.

And 40 minutes later,

in the silence
of their inactivity,

they open the door to history.

♪ ♪

(faint chirp)

A powerful gravitational wave
rumbles through both detectors,

Louisiana and Washington.

Had Robert Schofield worked
40 more minutes that night,

with the instruments
in test mode,

a signal that had been
on its way for 1.3 billion years

would never have been recorded.

SCHOFIELD:
I like to say,

you know, one of my biggest
contributions to LIGO

has been my laziness that day.

(indistinct conversations)

I got an email
from somebody here saying,

"Hey, look, look at this place
on the web."

(chirps)

I looked at that
and I said, "Holy (bleep)!"

♪ ♪

(chirps)

THORNE:
It was so strong

that you could see it by eye
in the data.

It was too good to be true.

LEVIN:
But it was true.

In fact it was loud,
and surprisingly clear.

And it just sang at you.

There it was, standing out.

LEVIN:
The signal lasted
less than a second,

but in that briefest of moments

it delivered
a cosmically profound message

more than a billion years
in the making,

proving the existence
of black holes.

THORNE:
So what we saw in the signal

involved oscillations of the
mirrors that were slow at first,

became faster and faster
and faster.

And this was precisely
the kind of behavior

that you would expect
from gravitational waves

caused by two black holes
going around each other,

spiraling together.

LEVIN:
Two massive black holes,

one 29 times
the mass of the sun,

the other 36 times
the mass of the sun,

whipping around each other
hundreds of times a second,

finally completing their act of
mutual destruction by merging...

Creating a single, larger
black hole of 62 solar masses.

The violent merger
converts some of the mass

into an apocalyptic release
of energy

beyond anything
ever before witnessed.

THORNE:
The collision, in effect,

creates a very-- a veritable
storm in the fabric or the shape

of space and time,

as though you had taken
three suns,

you had annihilated them
completely,

converted it
into gravitational waves.

The power was 50 times higher
than the output power

of all the stars
in the universe put together--

in a fraction of a second.

But the most powerful explosion

that humans have ever had
any evidence for

with the exception
of the Big Bang.

♪ ♪

LEVIN:
Since that very first signal
in September 2015,

LIGO has detected several more
collisions of black holes.

In October 2017,
Rai Weiss, Kip Thorne,

and LIGO's former director
Barry Barisch

received the Nobel Prize.

The LIGO discoveries prove
that black holes can merge--

one way they can grow bigger
quickly.

More and more evidence of these
merging black holes tells us

there are a lot of these
stellar black holes around,

that they can find each other
and, and merge.

LEVIN:
And the discovery opened
an entirely new way

of observing the universe.

♪ ♪

(chirp)

We always thought of astronomy

as an observational field

where we are looking
at radiation.

We are seeing things.

But this is not radiation.

This is something much more
fundamental.

These are sort of fundamental
tremors in space-time itself.

We can now hear the universe.

♪ ♪

LEVIN:
For the first time,

astronomers have simultaneously
seen and heard a cosmic event.

♪ ♪

In August 2017, LIGO detected
gravitational waves

from a collision
of two neutron stars.

Black holes are empty space,

but neutron stars
are dense dead stars

that can crash together
and light up the skies.

♪ ♪

When telescopes and satellites
around the globe

pointed in the direction
of the sound,

the world saw fireworks

in an explosive collision
and afterglow.

Possibly, the collision resulted
in the creation

of a new black hole.

But unless we observe
the formation of a black hole,

there is much
we will never know.

Because so much
about black holes

is irretrievably
out of our reach,

we can never know
where they came from,

what's inside, or their history.

♪ ♪

(explosion roars)

But we can imagine their future.

The number of black holes
in the universe is increasing.

And they're getting bigger.

Stars collapse,

black holes feed and merge,

new ones form.

Could it be that one day,

everything will end up
inside them

and they will rule the universe?

♪ ♪

Untold trillions upon trillions
of years after this happens,

and the last bits of matter
cross their event horizons,

black holes themselves
may radiate away

and vanish from this reality.

♪ ♪

Their mysteries are many,
and we're just starting

to unlock the secrets of these
strange, powerful places.

But one thing is certain.

Black holes will continue
to intrigue us,

tantalize us,

and challenge both our science
and our imaginations.

♪ ♪

♪ ♪

This "NOVA" program
is available on DVD.

To order, visit shopPBS.org
or call 1-800-PLAY-PBS.

"NOVA" is also available
for download on iTunes.

♪ ♪