galaxies astronomy 315 professor lee carkner lecture 20

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Galaxies Astronomy 315 Professor Lee Carkner Lecture 20

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Page 1: Galaxies Astronomy 315 Professor Lee Carkner Lecture 20

Galaxies

Astronomy 315Professor Lee

CarknerLecture 20

Page 2: Galaxies Astronomy 315 Professor Lee Carkner Lecture 20

The Size of the Universe

Separate star systems like the Milky Way or just nebula in our galaxy?

In the 1920’s Edwin Hubble used the new 100 inch Mt. Wilson telescope to view Cepheids in “spiral nebula” and found they were too distant to be in our galaxy

Page 3: Galaxies Astronomy 315 Professor Lee Carkner Lecture 20

Types of Galaxies A visual inspection reveals 3 types: Spiral

Elliptical

Composed of older stars Irregular

Look like altered spirals

Page 4: Galaxies Astronomy 315 Professor Lee Carkner Lecture 20

Spiral Galaxies Spiral galaxies are similar to the Milky

Way

Spiral arms contain gas and dust and young stars

We see a lot of spirals (~80% of bright

galaxies) Most smaller than the Milky Way

Page 5: Galaxies Astronomy 315 Professor Lee Carkner Lecture 20

Classifying Spiral Galaxies Spiral galaxies are classified based on two properties:

From this Hubble produced 3 categories: Sa

Sb

Sc

Loosely wound arms, small bulge

Page 6: Galaxies Astronomy 315 Professor Lee Carkner Lecture 20

M31, The Andromeda Galaxy (Sb)

Page 7: Galaxies Astronomy 315 Professor Lee Carkner Lecture 20

M83 (Sc)

Page 8: Galaxies Astronomy 315 Professor Lee Carkner Lecture 20

M100 (Sc)

Page 9: Galaxies Astronomy 315 Professor Lee Carkner Lecture 20

M51, The Whirlpool Galaxy (Sc)

Page 10: Galaxies Astronomy 315 Professor Lee Carkner Lecture 20

NGC 891 -- Edge-on Spiral

Page 11: Galaxies Astronomy 315 Professor Lee Carkner Lecture 20

Other Spirals Many spiral galaxies show a bar of material

across the nucleus (barred spiral) Milky Way has a bar

Some galaxies have disks and bulges, but no spiral arms (called S0 or lenticular)

Why do spirals look the way they do?

Sa to Sb to Sc is moving towards “diskier” galaxies with more star formation

Page 12: Galaxies Astronomy 315 Professor Lee Carkner Lecture 20

M95 -- Barred Spiral (SBb)

Page 13: Galaxies Astronomy 315 Professor Lee Carkner Lecture 20

NGC 1300 -- Barred Spiral (SBc)

Page 14: Galaxies Astronomy 315 Professor Lee Carkner Lecture 20

M102 -- S0 Spiral

Page 15: Galaxies Astronomy 315 Professor Lee Carkner Lecture 20

Elliptical Galaxies Elliptical galaxies have almost no structure

Classified by how elongated they look from

our point of view

Have almost no gas, dust or young stars

Have a wide range in size

Page 16: Galaxies Astronomy 315 Professor Lee Carkner Lecture 20

M87 -- Giant Elliptical (E1)

Page 17: Galaxies Astronomy 315 Professor Lee Carkner Lecture 20

M59 -- E5 Elliptical

Page 18: Galaxies Astronomy 315 Professor Lee Carkner Lecture 20

Irregular Galaxies

Some galaxies have no discernable regular shape

Often show evidence of star formation

Distortion might be due to: Galaxy collisions

Page 19: Galaxies Astronomy 315 Professor Lee Carkner Lecture 20

The Large Magellanic Cloud

Page 20: Galaxies Astronomy 315 Professor Lee Carkner Lecture 20

Hubble’s Tuning Fork

Hubble categorized the galaxies and then placed them on a diagram

As you go from left to right in the diagram you roughly increase in gas, dust, number of young stars and star formation rates

Page 21: Galaxies Astronomy 315 Professor Lee Carkner Lecture 20

Hubble’s Tuning Fork Diagram

Page 22: Galaxies Astronomy 315 Professor Lee Carkner Lecture 20

Galactic Collisions Galaxies should collide fairly often

What happens when they collide? May trigger wave of star formation

One galaxy may merge with another (galactic cannibalism)

Page 23: Galaxies Astronomy 315 Professor Lee Carkner Lecture 20

Evolution of Galaxies It is not completely clear how galaxies evolve,

but there is growing evidence for this basic picture

Burst uses up all gas and dust and star formation stops (Elliptical)

Page 24: Galaxies Astronomy 315 Professor Lee Carkner Lecture 20

Next Time Read Chapter 24.4-24.5