Astr 5460 Fri., Feb. 7, 2003
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Today: WIRO: Tonight! |
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Reminders/Assignments |
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Longair, Ch. 2 (Large Scale Struct.) |
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Start Longair, Ch. 3 (Galaxies) |
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Unless noted, all figs and eqs from Longair. |
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WIRO -- logistics
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We will leave after colloquium, about
5PM. Sabrina and I are driving. |
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Bring food and drinks (only water will
be available at WIRO). We can stop on
the way if necessary, but better to get early. |
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Dress WARMLY! Overkill is OK. |
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May stay until morning if weather is
good. Beds are available at WIRO. |
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WIRO – science+
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Mike Pierce is putting on the Prime
Focus camera (see webpage for more info). |
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Jon Darnel has one project with Chip
K. M33 blue imaging, 1-2 hours. |
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Pretty 3-color pictures for a calendar
– bring targets! Note that there is no
internet connection right now. |
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I’m working on developing a good
project. |
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Group Assignment: Take notes and
develop a WIRO/PFC Observer’s Handbook. |
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Reminders/Preliminaries
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Astro-ph preprints: |
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http://xxx.lanl.gov/astro-ph |
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Discuss homework assignments (briefly!) |
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Redshifted BB curve |
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MAP, PLANCK (Kiminki) |
Hubble’s Law and
Expansion
Hubble’s Law and
Expansion
Hubble’s Law and
Expansion
Hubble’s Law and
Expansion
Hubble’s Law and
Expansion
Hubble’s Law and
Expansion
Hubble’s Law and
Expansion
Hubble’s Law and
Expansion
Conclusions
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On the largest scales it is appropriate
to impose the conditions of isotropy and homogeneity, plus uniform expansion. |
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These simplifications plus GR provide
relatively simple “world models” that provide a framework for cosmology and
the origin of galaxies and other large scale structures. |
Chapter 3: Galaxies
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General, basic properties outlined
here. More will be covered in ASTR
5440. |
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Classifications |
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Luminosity Functions |
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Galaxy Masses |
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Elliptical Galaxies |
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Spiral Galaxies |
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Correlations with Types |
“Tuning Fork” Diagram
Spiral types
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The nuclear bulge is population II (old stars) |
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So the Sa – Sc sequence is consistent
with
little gas Þ more gas |
Elliptical Galaxy: M87
Irregular Galaxies:
Magellanic Clouds
More on Classifications
Frequency of Galaxy Types
Frequency of Galaxy Types
Frequency of Galaxy Types
The Local Group of
Galaxies
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Galaxies live in clusters |
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Rich clusters: thousands of galaxies |
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Poor clusters: Fewer than a thousand |
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The Coma Cluster
Interacting Galaxies: The
Antennae
Interacting Galaxies:
Cartwheel
Effects of Collisions
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Stars pass “through” each other,
although orbits disrupted |
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Gas clouds collide |
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Gas stripped away from stars |
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Collisions cause bursts of star
formation |
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Ellipticals may be galaxies which have
suffered collisions |
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Spirals may be galaxies which have not
suffered collisions |
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Joshua Barnes (Hawaii) and the Space
Telescope Science Institude provide a simulation of the Antenna Galaxies: http://imgsrc.stsci.edu/op/pubinfo/pr/1997/34/images/anima.mov |
Simulation of the
Cartwheel Encounter
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From the Space Telescope Science
Institute which also provided the Cartwheel image in the textbook: |
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http://imgsrc.hubblesite.org/hu/discoveries/striking_encounters/graphics/cartwheel.mpg |
Luminosity Functions