How far away is it?
To gain an understanding of the scale of the Universe you can make a scale model the size of a city.
To Do and Notice
Draw a city avenue named Universe Avenue.
Let it run for 14 blocks. Assume each block is 100 meters long.
The Universe that we see from earth reaches out 14
Billion light years to the big bang.
(The best guess in 2004 is 13.7 Billion light years with an uncertainty of plus or minus 0.2 billion light years)
Each block represents a billion light years. So, a million light years is 10 cm.
Look down at your feet. Our galaxy, the Milky Way
is there,100,000 light years in diameter.
In our model it is smaller than a dime, since in our model, 100,000 light years is 1 centimeter.
The galaxy has a central bulge about 10% as thick as the diameter.
In our model the central bulge is 1 mm thick, the thickness of a dime.
The disk of the galaxy is thin, about a third as thick as the bulge.
In our model it is five times thicker than a hair.
The nearest large galaxy to us is the Andromeda galaxy it is 2 Million light years away.
So the Andromeda galaxy is a second dime located or 20 cm or one handspan away.
The Milky Way and the Andromeda galaxies are the
largest two members of the local group of galaxies. The local group
is a cluster of about 20 galaxies within 3 million light years.
20 dimes within a sphere 30 centimeters in diameter, within a sphere the size of a basketball.
The nearest group of galaxies is the Sculptor Group, with six bright spirals, it is 7 million light years away, or 70 cm. The galaxies in the sculptor group are all within a 3 million light year diameter, also within a basketball sized sphere (30 cm in diameter).
Further away is the Virgo cluster of galaxies, it contains over 10,000 galaxies. That's a lot of coins! It is 45 million light years away, 4.5 meters away in out model, the length of a car. It is a sphere of galaxies 80 cm in diameter the size of a giant pumpkin.
Our local group of galaxies, the sculptor group and the Virgo cluster are members of a larger organization of galaxies called a supercluster.
Our supercluster is centered on the Virgo cluster and is roughly spherical with a diameter of about 100 million light years or 10 meters in our model. So it is a 10 meter diameter sphere centered 4.5 meters away. We are near the edge. It contains millions of galaxies. The McBean theater at the Exploratorium is one eighth of a 10 meter diameter sphere, picture it full of basketball sized groups of dozens of coin-size galaxies and of giant pumpkin sized clusters of tens-of thousands of galaxies.
Superclusters are the largest spherical groupings in the universe.
If we look for structures that span 3 blocks in our model, 3 billion light years spheres, we find that a single three block cube neighborhood of the universe is pretty much like every other three block cube. The universe is homogeneous, the same, from one three block group to the next. It is also isotropic, meaning it looks the same in all directions.
Superclusters are organized into larger structures that form long filaments or walls, there are also huge empty regions devoid of superclusters
The most distant known objects of their kind.
The most distant Cepheid variable whose distance has been measured by the Hubble telescope is in a galaxy 108 million light years away, named NGC 4603. A tenth of a block or 10 meters distant. Twice as far as the center of the Virgo cluster.
The most distant supernova of type 1a, which was
measured by the Hubble telescope in 2001, has a redshift, z, of
The redshift is the ratio of the change in wavelength of light as it traveled through the expanding universe to its original wavelength z = Dl/l .
The distance to this supernova can be measured because its brightness is known, its distance is 10 billion light years, or 10 blocks in our model.
The furthest galaxy clusters imaged by the Hubble telescope are estimated to be 12 billion light years, or 12 blocks, away.
The most distant object seen by the Hubble telescope is a distant galaxy imaged by the gravitational bending of light by a less distant distant cluster of galaxies. It's redshift is 5.5 and its distance is estimated to be 13.2 billion light years, just 500,000 light years from the big bang.
Radio telescopes can see further, they can see the
edge of the big bang, the time when it became transparent,. Just
300,000 light years shy of the big bang itself.
A few dime diameters from the edge.
The City Universe
Object Distance to its center Scale distance to its center Diameter Scale diameter Milky Way galaxy 0 0 100,000 LY 1 cm Andromeda Galaxy 2 million LY 20 cm 100,000 LY 1 cm Local Group 20 galaxies 0 0 3 million LY 30 cm Sculptor Group 30 galaxies 7 million LY 70 cm 3 million LY 30 cm Virgo Cluster 10,000 galaxies 45 million LY 4.5 m 8 million LY 80 cm Local Supercluster 45 million LY 4.5m 100 million LY 10m Most distant cepheid 100 million LY 10 m redshift Most distant supernova 1a 11 billion LY 1100 m or 11 blocks z = 1.7 Most distant galaxy (gravity lensed) 13 billion LY 1,300 m or 13 blocks z = 5 Most distant galaxy cluster 12 billion LY 1,200 m or 12 blocks Most distant quasar 13.2 billion LY 1320 m or 13.2 blocks z = 5.5 big bang visible edge 14 billion LY 1,400 m or 14 blocks z = 1300
Distance to its center
Scale distance to its center
Milky Way galaxy
2 million LY
Local Group 20 galaxies
3 million LY
Sculptor Group 30 galaxies
7 million LY
3 million LY
Virgo Cluster 10,000 galaxies
45 million LY
8 million LY
45 million LY
100 million LY
Most distant cepheid
100 million LY
Most distant supernova 1a
11 billion LY
1100 m or 11 blocks
z = 1.7
Most distant galaxy (gravity lensed)
13 billion LY
1,300 m or 13 blocks
z = 5
Most distant galaxy cluster
12 billion LY
1,200 m or 12 blocks
Most distant quasar
13.2 billion LY
1320 m or 13.2 blocks
z = 5.5
big bang visible edge
14 billion LY
1,400 m or 14 blocks
z = 1300
What's Going On?
What we measure for an object is its redshift, usually given the symbol z, where z = Dl/l, the change in wavelength, Dl, divided by the initial wavelength, l.
The redshift of a distant object is due to the
expansion of the universe, the emitted photon of light has a
wavelength that increases as it travels through the expanding
universe. So a galaxy seen at a redshift of 0.1 means that the
universe has expanded by 10% since the light from that galaxy was
emitted. It also means that the universe was
1- 0.1 = 0.9 as old then as it is now. At these relatively close distances a redshift of 0.1 means a distance equal to about a tenth the distance to the big bang, which we now think is 14 billion light years, a tenth of this would be 1.4 billion light years, or 1.4 blocks away in our model.
However for larger redshifts we have to use more complex equations to calculate the fraction of the age of the universe that has passed since the light was emitted. See the Math Root.
A galaxy with a redshift of 1 means that the wavelength of light has doubled since it was emitted, and so the Universe has doubled since the time of emission.
What astronomers actually measure for distant galaxies is their redshift, z, not their distance.
To find the expansion of the distance now, dnow between two galaxies initially at distance dthen when one is seen from the other to have redshift z the equation is dnow = dthen (1+z). We see a galaxy with a redshift 1 at a time when distances between galaxies in the universe were half what they are today. Said another way, the universe has doubled in size since the light was emitted, and so has the wavelength of the light.
We see the galaxy at a redshift z when it was some
fraction, f, of the age of the universe, T.
The best current estimate for the age of the universe, T is 14 billion years (actually 13.7+-0.2 billion years.
)The exact equation to calculate f when we know z depends on the model we choose for how the universe has expanded.
If gravity is slowing the universe so rapidly that it will eventually stop and recollapse it is called a closed universe.
If gravity will never stop the universe from expanding it is said to be open,
and if it is delicately balanced between these two options, so that it will expand forever while slowing toward zero growth at infinite time it is said to be flat.
Data indicates that throughout most of its
expansion the universe has been approximately flat.
For a flat universe the fraction f is
f = 1/(1+z)3/2
So a galaxy of redshift z = 0.1 is seen when the
universe was a fraction f = 1/(1+0.1)3/2 of its current
This is f = 1/(1.15) = 0.85 which, to one significant digit, is equal to 0.9 as we said above.
Light from a galaxy at a redshift of 1 left the galaxy when the universe was
f = 1/23/2 = 0.35 thirty five percent
of its current age, or 5 billion years.
It is therefore 14 - 5 = 9 billion light years away.
Light with a redshift of 5 representing some of the most distant galaxies seen left when the universe was
f = 1/63/2 = .07 of its current age just under a billion years old. It is therefore 13 billion light years away.
(Note all of these distance were taken from observations up to 2001.)
The distance to the most distant Cepheid, Supernova, galaxy, galaxy cluster, and quasar change on a monthly basis. Use the ineternet to update the table above to keep up with the most recent observations.
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Scientific Explorations with Paul Doherty
30 April 2001