Download Chap 16: Galaxies

Chapter 16
Galaxies
Guidepost
Our Milky Way Galaxy is only one of the many billions
of galaxies visible in the sky. This chapter will expand
your horizon to discuss the different kinds of galaxies
and their complex histories. Here you can expect
answers to five essential questions:
• What do galaxies look like?
• How do astronomers measure the distances to
galaxies?
• Do other galaxies contain supermassive black holes
and dark matter, as does our own galaxy?
• Why are there different kinds of galaxies?
Guidepost (continued)
As you begin studying galaxies, you will discover they
are classified into different types, and that will lead you
to insights into how galaxies form and evolve. It will
also answer an important question about scientific
methods:
• How does classification help scientists understand
nature?
In the next chapter, you will discover that some
galaxies are violently active, and that will give you
more clues to the evolution of galaxies.
Outline
I. The Family of Galaxies
A. The Discovery of Galaxies
B. How Many Galaxies are there?
C. The Shapes of Galaxies
II. Measuring the Properties of Galaxies
A. Distance
B. The Hubble Law
C. Diameter and Luminosity
D. Mass
E. Supermassive Black Holes in Galaxies
F. Dark Matter in Galaxies
G. Gravitational Lensing and Dark Matter
Outline (continued)
III. The Evolution of Galaxies
A. Clusters of Galaxies
B. Colliding Galaxies
C. The Origin and Evolution of Galaxies
D. The Farthest Galaxies
Galaxies
• Star systems like our Milky Way
• Contain a few thousand to tens of billions (10121013)of stars.
• Large variety of shapes and sizes
Galaxy Diversity
Even seemingly
empty regions
of the sky
contain
thousands of
very faint, very
distant galaxies
Large variety of
galaxy
morphologies:
Spirals
Ellipticals
Irregular
(some interacting)
The Hubble Deep Field:
10-day exposure on an apparently empty field in the sky
Galaxy Classification
Ellipticals:
E0, …, E7
E0 =
Spherical
Spirals:
Sa
Large
nucleus;
tightly
wound arms
E1
Sb
Sc
E7 = Highly
elliptical
E6
Small
nucleus;
loosely
wound arms
Gas and Dust in Galaxies
Spirals are rich in
gas and dust
Ellipticals are almost
devoid of gas and dust
Galaxies with disk and bulge,
but no dust are termed S0
Barred Spirals
• Some spirals show a
pronounced bar structure
in the center
• They are termed
barred spiral galaxies
• Sequence:
SBa, …, SBc,
analogous to regular
spirals
Irregular Galaxies
Often: result of galaxy
collisions / mergers
Often: Very active star formation
(“Starburst galaxies”)
The Cocoon
Galaxy
NGC 4038/4039
Some: Small (“dwarf galaxies”)
satellites of larger galaxies
(e.g., Magellanic Clouds)
Large
Magellanic
Cloud
Distance Measurements to Other
Galaxies (1)
a) Cepheid Method: Using Period – Luminosity relation
for classical Cepheids:
Measure Cepheid’s Period  Find its luminosity 
Compare to apparent magnitude  Find its distance
b) Type Ia Supernovae (collapse of an accreting white
dwarf in a binary system):
Type Ia Supernovae have well known standard
luminosities  Compare to apparent magnitudes 
Find its distances
Both are “Standard-candle” methods:
Know absolute magnitude (luminosity)  compare to
apparent magnitude  find distance.
Cepheid Distance Measurement
Repeated
brightness
measurements
of a Cepheid
allow the
determination
of the period
and thus the
absolute
magnitude.
 Distance
Distance Measurement
Using Type Ia Supernovae
Remember: Type Ia supernovae
(collapse of an accreting white dwarf)
have almost uniform luminosity →
Absolute magnitude
Observe
apparent
magnitude 
Distance
The Most Distant Galaxies
At very large
distances, only
the general
characteristics
of galaxies can
be used to
estimate their
luminosities 
distances.
Cluster of galaxies at ~ 4 to 6 billion light years
Distance Measurements to Other
Galaxies (2): The Hubble Law
E. Hubble (1913):
Distant galaxies are moving away from our Milky Way, with
a recession velocity, vr, proportional to their distance d:
vr = H0*d
H0 ≈ 70 km/s/Mpc
is the Hubble
constant
• Measure vr
through the
Doppler effect 
infer the distance
The Extragalactic Distance Scale
• Many galaxies are typically millions or
billions of parsecs from our galaxy.
• Typical distance units:
Mpc = Megaparsec = 1 million parsec
Gpc = Gigaparsec = 1 billion parsec
• Distances of Mpc or even Gpc  The
light we see left the galaxy millions or
billions of years ago!!
• “Look-back times” of millions or billions of years
Galaxy Sizes and Luminosities
Vastly different sizes
and luminosities:
From small, lowluminosity irregular
galaxies (much
smaller and less
luminous than the
Milky Way) to giant
ellipticals and large
spirals, a few times
the Milky Way’s
size and luminosity
Rotation Curves of Galaxies
From blue / red shift of spectral
lines across the galaxy
 infer rotational velocity
Observe frequency of
spectral lines across a
galaxy.
Plot of rotational velocity
vs. distance from the
center of the galaxy:
Rotation Curve
Determining the Masses of Galaxies
三條不同波長
的譜線顯現一
樣的 rotation
curve
波長
Based on rotation curves, use Kepler’s 3rd law to infer
masses of galaxies
Masses and Other Properties of
Galaxies
Supermassive Black Holes
From the
measurement of
stellar velocities
near the center of
a galaxy:
Infer mass in the
very center 
central black
holes!
Several million,
up to more than a
billion solar
masses!
 Supermassive
black holes
Dark Matter
Adding “visible” mass in:
• stars,
• interstellar gas,
• dust,
…etc., we find that most of the mass is “invisible”!
• The nature of this “dark matter” is not
understood at this time.
• Some ideas: brown dwarfs, small black holes,
exotic elementary particles.
Gravitational Lensing
According to General Relativity, light will be bent
towards a massive object when passing it.
This phenomenon is called Gravitational Lensing
It can be used to detect otherwise invisible
Dark Matter and measure its mass.
Clusters of Galaxies
Galaxies generally do not exist in isolation,
but form larger clusters of galaxies.
Rich clusters:
Poor clusters:
1,000 or more galaxies,
diameter of ~ 3 Mpc,
condensed around a large,
central galaxy
Less than 1,000 galaxies
(often just a few),
diameter of a few Mpc,
generally not condensed
towards the center
Our Galaxy Cluster: The Local Group
M31: 仙女座
大星雲系
Milky Way
Small Magellanic
Cloud
Large Magellanic
Cloud
Andromeda
galaxy
Neighboring Galaxies
Some galaxies of our local group are difficult to
observe because they are located behind the
center of our Milky Way, from our view point.
The Canis Major Galaxy
The Canis Major Dwarf Galaxy has
orbited around the Milky Way a number
of times, and tidal forces have ripped
away stars and gas.
Interacting Galaxies
Cartwheel Galaxy
Particularly in rich
clusters, galaxies can
collide and interact.
Galaxy collisions
can produce
ring galaxies and
NGC 4038/4039
tidal tails.
Often triggering active
star formation:
starburst galaxies
Tidal Tails
Example for galaxy
interaction with tidal tails:
The Mice
Computer simulations
produce similar
structures.
Simulations of Galaxy Interactions
Numerical
simulations
of galaxy
interactions
have been
very
successful
in
reproducing
tidal
interactions
like bridges,
tidal tails,
and rings.
Mergers of Galaxies
NGC 7252:
Probably result
of merger of
two galaxies,
about one
billion years
ago:
Small galaxy
remnant in the center
is rotating backward!
Radio image of M 64: Central
regions rotating backward!
Multiple
nuclei in giant
elliptical
galaxies
Interactions of Galaxies
with Clusters
When galaxies pass through the thin gas of their
home cluster, their own gas can be almost
completely stripped away.
Starburst Galaxies
Starburst galaxies: Galaxies in which stars are
currently being born at a very high rate.
Starburst galaxies contain many young stars
and recent supernovae, and are often very
rich in gas and dust; bright in infrared:
ultraluminous infrared galaxies
The Farthest Galaxies
The most distant galaxies visible by HST are seen at a
time when the universe was only ~ 1 billion years old.
Mid-term make-up question
by 蘇恩寧
Q: The first question of our mid-term exam tells us that the
farthest star can be seen by naked eyes should be 5167
light years away. Why are we able to see Andromeda
galaxy (M31) which is about 2.54 million light years
away without aid when the night sky is clear?
A: Surely we can’t see a star which is 2.54 million light years
from us, but obviously Andromeda galaxy itself isn’t a star
but is made up of a great amount of stars. We can consider
a galaxy as a very big star, which is much bigger (high
diameter) than a single star so that the light intensity is also
higher. [not completely wrong, but not necessary true: Just
because of the great distance between us and Andromeda
galaxy we can’t distinguish between 2 single stars in the
galaxy even with a telescope.]