Download Galaxies and Active Galaxies

Chapter 25: Galaxies
What are galaxies?
How are they distributed in space?
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Discovery of other Galaxies
• Using large telescopes one can see clouds of dust and gas inside the
Galaxy.
• One can also see other peculiar milky nebulae scattered among the
stars.
• Some of these milky nebulae have spiral shapes
• Others look like squashed spheres or tortured messes of material.
• Three of the milky nebulae are visible as fuzzy patches to the naked
eye:
– one is in the constellation Andromeda
– two others (called the Large and Small Magellanic Clouds after the first
European explorer to see them, Ferdinand Magellan) are in the southern sky in
the constellations Mensa and Hydrus.
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Galaxies Discovery Pioneers
• Work by
– Edwin Hubble (lived 1889--1953)
– Milton Humason (lived 1891--1972)
– in the 1930's established that each of the
spiral nebulae was another huge star system,
called a galaxy
• Galaxy is from the Greek ``galactos'',
meaning ”milk”.
• Hubble and Humason used large high
resolution telescopes to measure the
distances to the galaxies.
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Other Galaxies
• Galaxies are
– organized systems
– thousands to hundreds of thousands of light
years across
– made of tens of millions to trillions of stars
– sometimes mixed with gas and dust all held
together by their mutual gravity.
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Star Count in a Galaxy
– One gets an estimate of the number of stars in a
galaxy by dividing the total luminosity of the galaxy
by a typical star's luminosity.
– A more accurate value would result if you use the
galaxy's luminosity function (a table of the
proportion of stars of a given luminosity).
– Or you could divide the total mass of the galaxy by
a typical star's mass (or use the mass function to
get the proportions right).
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Distances to other Galaxies
• Distances between galaxies are large and are often
measured in megaparsecs.
• A megaparsec is one million parsecs
– or about 3.3 million light years.
• Example:
– distance between the Milky Way and the closest large
galaxy, the Andromeda Galaxy, is about 0.899
megaparsecs.
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Shapley-Curtis debate
– Big controversy in the 1910's and early 1920's over whether the
nebulae called galaxies were outside the Milky Way or were
part of it.
– National Academy of Sciences held a debate between the opposing
sides in 1920.
– Those favoring a large Milky Way with the spiral nebulae inside it
were represented by Harlow Shapley.
– Those favoring the spiral nebulae as separate groups of stars
outside the Milky Way were represented by Heber Curtis.
– The Shapley-Curtis debate did not decide much beyond the fact
that both sides had powerful evidence for their views.
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Resolution
• Edwin Hubble and Milton Humanson set out to
resolve the debate
– by using the largest telescope at the time,
– the 100-inch telescope on Mount Wilson,
– to study the large spiral nebula in the Andromeda
constellation.
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Resolution (2)
– Because of its large mirror, the telescope had sufficient resolving
power and light-gathering power to spot individual stars in the
Andromeda Galaxy.
– In the mid-1920's they discovered Cepheid variables in the galaxy
and used the period-luminosity relation to find that the distance to
the galaxy was very much greater than even the largest estimates
for the size of the Milky Way.
– Galaxies are definitely outside the Milky Way and our galaxy is
just one of billions of galaxies in the universe.
– Their discovery continued the process started by Copernicus long
ago of moving us from the center of the universe.
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Types of Galaxies
• Edwin Hubble divided the galaxies into
three basic groups:
– ellipticals,
– spirals,
– irregulars.
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Types of Galaxies (2)
–
–
–
–
Ellipticals are smooth and round or elliptical.
Spirals are flat with a spiral pattern in their disk.
Irregulars have stars and gas in random patches.
Most galaxies are small and faint so only the
luminous galaxies are seen at great distances.
– Very luminous galaxies tend to be either the elliptical
or spiral type, so they are the ones often displayed
in astronomy textbooks.
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Sequence of
Galaxy Classification
• Hubble (1936) put
these groups onto a
two-pronged sequence
that looks like a tuning
fork.
• He thought
(incorrectly) that
galaxies evolved from
left to right in diagram.
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Not All Ideas are Correct…
• Astronomers now know that it is NOT an
evolutionary sequence because each type of galaxy
has very old stars.
• The oldest stars in any galaxy all have about the
same age of around 15 billion years.
• This means that spirals form as spirals, ellipticals
form as ellipticals, and irregulars form as irregulars.
• However, the “tuning fork” diagram remains
convenient for classifying galaxies.
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Ellipticals
• Smooth and elliptical in appearance.
• Have four distinguishing characteristics:
– much more random star motion than orderly
rotational motion
• star orbits are aligned in a wide range of angles and have a
wide range of eccentricities.
– Little dust and gas left between the stars
– No new star formation occurring now and no hot,
bright, massive stars in them.
– No spiral structure.
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Elliptical Sub-classification
• Most elliptical galaxies are small and faint.
• The dwarf ellipticals may be the most common type
of galaxy in the universe
– (or maybe the dwarf irregulars are).
• Examples of elliptical galaxies are M32 (an E2
dwarf elliptical next to the Andromeda Galaxy) and
M87 (a huge elliptical in the center of the Virgo
cluster).
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Elliptical Galaxies – Example 1
• Messier 32: a dwarf
elliptical (E2) satellite
galaxy of the
Andromeda Galaxy.
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Elliptical Galaxies – Example 2
• Messier 87:
– giant elliptical (E1)
– at the core of the Virgo
Cluster
– Grown very large by ``eating''
other galaxies.
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Elliptical Galaxies – Example 3
• Leo I:
– dwarf elliptical
– E3
– Local Group.
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Elliptical Galaxies – Example 4
• Messier 110
– dwarf elliptical
– E6
– satellite of Andromeda Galaxy.
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Spiral Galaxies
• Flattened disks with a spiral pattern in
the disk.
• Spiral arms can go all of the way into the
bulge or be attached to the ends of a
long bar of gas and dust that bisects the
bulge.
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Spiral Galaxies Characteristics
• Four distinguishing characteristics of the
spirals are:
1. More orderly, rotational motion than random motion
• the rotation refers to the disk as a whole and means that
the star orbits are closely confined to a narrow range of
angles and are fairly circular.
2. Lot of gas and dust between the stars.
3. New star formation occurring in the disk,
particularly in the spiral arms.
4. A spiral structure.
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Spiral Galaxies – Example 1
• Andromeda Galaxy
–
–
–
–
M31
large spiral galaxy (Sb)
near the Milky Way.
Note
• M32 just above it
• M110 below it.
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Spiral Galaxies – Example 2
• Triangulum Galaxy
• M33
• Small spiral galaxy
(Scd)
• in the Local Group.
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Spiral Galaxies – Example 3
• Messier 81
• Large spiral galaxy (Sb).
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Spiral Galaxies – Example 4
• NGC 2997
• Large face-on
spiral galaxy (Sc).
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Spiral Galaxies – Example 5
• NGC 1365
– barred spiral galaxy
(SBbc).
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Spiral Galaxies – Example 6
• NGC 3351
• (M95)
• Barred spiral galaxy
(SBb).
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Irregular Galaxies
• Irregular galaxies have no definite structure.
• Stars bunched up but the patches are randomly
distributed throughout the galaxy.
• Some irregulars have a lot of dust and gas so
star formation is possible.
• Some are undergoing a burst of star formation
“now”, many H II regions are seen in them.
• Others have very little star formation going on
in them (even some of those with a lot of gas
and dust still in them).
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Irregular Galaxies (2)
• Most irregulars are small and faint.
• The dwarf irregulars may be the most common type of
galaxy in the universe (or maybe the dwarf ellipticals are).
• Dwarf galaxies far away are faint and hard to see.
• Perhaps if the dwarf galaxies were brighter, E. Hubble
would have arranged the galaxies in a different sequence
instead of the two-pronged sequence.
• Examples of irregular galaxies are the Large and Small
Magellanic Clouds (two small irregulars that orbit the Milky
Way).
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Irregular Galaxies – Example 1
• Large Magellanic Cloud
– Dwarf irregular satellite
galaxy of the Milky Way.
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Irregular Galaxies – Example 2
• Small Magellanic
Cloud
– Dwarf irregular
satellite galaxy of
the Milky Way.
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Irregular Galaxies – Example 3
• NGC 6822
– Dwarf irregular galaxy in the
Local Group.
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Irregular Galaxies – Example 4
• IC 5152
– Dwarf irregular galaxy
in the Local Group.
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Irregular Galaxies – Example 5
• NGC 1313
– starburst galaxy
– also called a barred
spiral galaxy (SBc).
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Irregular Galaxies – Example 6
• Messier 82
– starburst galaxy.
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Distribution in the Sky
• Galaxies are distributed fairly uniformly across the
sky.
• Approximately the same number of galaxies are
seen in every direction
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More about Galaxy Distributions
• The distribution of galaxies is not perfectly smooth.
• They clump together into loose groups.
• Three-dimensional maps of the universe have
revealed surprisingly large structures in the universe.
• Galaxies like to group together and those groups, in
turn, congregate together.
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Distances To Galaxies
• As for the determination of stellar properties,
finding the distance to galaxies is essential for
comparing the galaxies against each other.
• In order to determine the luminosities and masses of
the galaxies and the distribution of the mass inside
the galaxies, one must know their distance from our
own Galaxy.
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Galaxy Distance Determination
• Use the period-luminosity relation of Cepheid variable stars
to derive the distance from the apparent brightness of the
Cepheids.
– Works only for the nearby galaxies.
• For galaxies farther away, other standard candle techniques
involving objects more luminous than Cepheids like
supernova explosions or supergiant stars are used.
– Luminosities are not as well known or uniform,
– Greater uncertainty in the derived distances to the very distant
galaxies.
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Distance and Redshift
• In 1914, Vesto Slipher (1870--1963) announced results from
spectra of over 40 spiral galaxies.
• He found that over 90% of the spectra showed redshifts
which meant that they were moving away from us.
• Edwin Hubble and Milton Humason found distances to the
spiral nebulae.
• When Hubble plotted the redshift vs. the distance of the
galaxies, he found a surprising relation:
– more distant galaxies are moving faster away from us.
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Hubble Law
• Hubble and Humason announced their result in 1931:
– the Galactic recession speed = H  distance,
– where H is a number now called the Hubble constant.
• This relation is called the Hubble Law and the Hubble
constant is the slope of the line.
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Determination of the Hubble Constant
• With distances measured in megaparsecs (Mpc) and
the recession speed in kilometers/second (km/sec),
the Hubble constant is between 60 and 70
km/sec/Mpc.
• Value found by using the galaxies that have accurate
distances measured (Cepheids, etc.) and dividing
their recession speeds by their distances.
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Benefits of the Hubble Law
• It is easy to find the recession speeds of galaxies from their
redshifts.
• The Hubble law provides an easy way to measure the
distances to even the farthest galaxies from the (recession
speed/H).
• For example, if a galaxy has a redshift of 20,000 km/sec and
H is set to 70 km/sec/Mpc, then the galaxy's distance =
(20,000 km/sec)/(70 km/sec/Mpc) = 20,000/70 ×
[(km/sec)/(km/sec)] Mpc = 286 megaparsecs.
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The Center of the Universe ?
• At first glance,
– it looks like the Milky Way is at the center of the
universe
– it committed some galactic social blunder because all of
the other galaxies are rushing away from it (there are a
few true galactic friends like the Andromeda galaxy that
are approaching it).
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Copernican principle
• Hubble law shows that there is actually not a violation of
the Copernican principle.
• More distant galaxies move faster.
• Galaxies (or galaxy clusters) are all moving away from each
other
• The universe is expanding uniformly.
• Every other galaxy or galaxy cluster is moving away from
everyone else.
• Every galaxy would see the same Hubble law.
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Expansion
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Masses of Galaxies
• Masses of galaxies are found from the orbital motion of
their stars.
• Stars in a more massive galaxy orbit faster than those in a
lower mass galaxy because the greater gravity force of the
massive galaxy causes larger accelerations of its stars.
• By measuring the star speeds, one finds out how much
gravity there is in the galaxy.
• Since gravity depends on mass and distance, knowing the
size of the star orbits enables you to derive the galaxy's
mass.
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Masses from Rotation Curve
for Spiral Galaxies
• The rotation curve shows how orbital speeds in a
galaxy depend on their distance from the galaxy's
center.
• The mass inside a given distance from the center =
(orbital speed)2 × (distance from the center)/G.
• Obital speed is found from the doppler shifts of the
21-cm line radiation from the atomic hydrogen gas.
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A Mass Problem
• The stars and gas in most galaxies move much quicker than expected
from the luminosity of the galaxies.
• In spiral galaxies, the rotation curve remains at about the same value
at great distances from the center (it is said to be “flat”).
• This means that the enclosed mass continues to increase even though
the amount of visible, luminous matter falls off at large distances from
the center.
• In elliptical galaxies, the gravity of the visible matter is not strong
enough to accelerate the stars as much as they are.
• Something else must be adding to the gravity of the galaxies without
shining.
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Dark Matter Problem
• That something else is called dark matter.
• It is material that does not produce detectable amounts of
light but it does have a noticeable gravitational effect.
• Astronomers are not sure what the dark matter is made of.
• Possibilities range from large things like planets, brown
dwarfs, white dwarfs, black holes to huge numbers of small
things like neutrinos or other particles that have not been
seen in our laboratories yet.
• The nature of dark matter is one of the central problems in
astronomy today.
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