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Mini Review:

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... CMB fit nicely with First peak and adiabatic model, but need MAP data to be sure ... A very neat confirmation of adiabatic initial fluctuations ... – PowerPoint PPT presentation

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Title: Mini Review:


1
  • Mini Review
  • Ocams Razor Start out with simplest
    assumptions
  • Hot Big Bang, Expanding Universe
  • Only baryonic matter gt
  • CMB existence, universe old and large and
    expanding

2
  • CMB too smooth
  • Add non-baryonic matter
  • Galaxies seen early (high 1z) gt CDM
  • First Peak in CMB indicates universe flat IF we
    put in model of initial fluctuations as
    adiabatic.
  • Wt 1, k 0
  • Second and Third peaks of CMB fit nicely with
    First peak and adiabatic model, but need MAP data
    to be sure

3
  • SNe says from a measure of the geometry of the
    universe versus time gt
  • Accelerating Universe gt Dark Energy
  • Clusters of galaxies say Wm lt 0.4 gt
  • With CMB Wt1, gt WL gt 0.6, gt Dark Energy
  • Dark Energy is the dark side of physics

4
  • Ways to overcome dark side
  • Assume SNe wrong
  • Assume Clusters wrong
  • Assume other new physics (e.g. iso-curvature) in
    early about 10-30 sec after BB rather than
    adiabatic fluctuations gt
  • In this case First peak doesnt require Wt 1, k
    0 flat in this case.
  • First Peak in CMB looks so solid need new
    interpretation for a model with no Dark Energy.
  • Cluster and SNe observations alone are less
    solid.

5
  • In early Universe, any goes so to a few,
    iso-curvature more appealing than adiabatic
  • First, Second and Third peaks are likely to be
    verified by MAP
  • A very neat confirmation of adiabatic initial
    fluctuations
  • Status quo is very likely to be upheld gt
  • Our final answer is Dark Energy, CDM, the
    Universe is flat but the expansion rate of the
    Universe is increasing

6
CMB peak plot
CMB smoothness map
7
(No Transcript)
8
End mini-Review, back to clusters
9
  • Some of missing mass was found, but not enough
    gt confirmation of non-baryonic dark matter
  • Second method
  • Use hot (100 million K) gas.
  • Most light comes out in X-rays.

10
X-ray
Optical
No color
False color
11
Concept of escape velocity
If an object is moving fast enough the object
will escape the pull of gravity of that system. gt
  • (1/2)mv2 gt GMm/R
  • m mass of escaping object
  • v velocity of escaping object
  • M mass of retaining object,
  • R distance from center to center

12
  • Atom mass is m (assumed)
  • Cluster mass is M
  • gt Measure T of gas
  • Relate T to v (simple theory)
  • Derive M!
  • Derived M agrees with galaxy velocity method

13
Bottom Line from first 2 methods
  • Gas mass 3-5 times total galaxy mass
  • Total directly detected baryonic matter
    (galaxies plus hot gas) mass still about 10
    (closer to 8) times too low! gt
  • Wouldnt hurt to check another way

OK check one more way! gt Gravitational lensing
14
Gravitational Lensing
Magnifies and distorts images
15
Gravitational Lensing
  • 4-d surface is distorted by local mass
    concentration
  • light travels on the surface
  • light path is deflected when traveling close to
    the body

Black hole
16
Gravitational Lensing Cont.
Gives rise to beautiful effects
Core of the Cluster called A2218
Arc-like structures caused by grav. lensing of
the mass in the cluster
17
Grav. Lensing
  • Derive a cluster mass again!
  • Agrees with other methods

18
  • Number of clusters there are per unit volume
  • lower bound on the Wm! about 0.1- 0.2 !
  • We will assume 0.1

19
Models of how clusters form and evolve yield
total Wm
20
Model of Cluster formation and Wm
  • Universe is expanding
  • Density falls
  • gt Total mass in a cluster radius is less than
    cluster mass. gt
  • Cant form any more clusters then.

21
  • Prediction
  • If we see a steep (factor of 2) in number of
    clusters per unit volume as go from z 0.1 to z
    1, then Wm gt 0.7
  • See shallow change (less than factor of 1.2),
    then Wm lt 0.4
  • See shallow change gt
  • Wm lt 0.4, all fits!

22
Clusters are no longer able to form as the
universe is not dense enough
High Wm
Low Wm
No. of clusters per unit volume
z
Age of universe
23

Clusters have problems also
Just measuring the mass is difficultgt
24
Velocity of galaxy measurement assumes you know
all the galaxies are in the clusters and how
they are moving.

And, where do clusters end (in radius), anyway?
Gas mass measurements based on possibly false
assumption of stable situation.
  • Our cluster counts could be wrong
  • Our model for relating Wm to number of clusters
    per unit volume with age of universe could be
    wrong
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