Particle Physicists and Astrophysicists working together

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Particle Physicists and Astrophysicists working
together?

• Simon White said in a recent paper By
  uncritically adopting the values of an alien
  system, astronomers risk undermining the
  foundations of their own current success and
  endangering the future vitality of their field.
  (Simon White Summer 2006, astroph)
• David Gross strongly disagreed.
• Is there a culture clash? Who is right? Is this
  conference ruining all of us in attendence???

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(Dunkley WMAP)
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• What I like about these parameters is that they
  confirm a theory Ive been using for years!
• Within errors our Universe is defined by
• h WDE 1 - Wtot 1/ v 2
  0.707
• (Joke)
• It much more satisfying that this CMB h agrees
  with the best number from the HST Hubble key
  project, as Saurabh Jha told us H0 73 6
  km/s/Mpc, but it was slightly disturbing that you
  get this answer by averaging two independent
  analyses of the same data! This actually
  continues a very long tradition in astrophysics
  (Sandage 50 vs. deVac 100!), but needs to get
  straightened out one of the these decades.
• Also we heard from Jha about the weird Hubble
  Bubble, something I hope will just go away.

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Summary Baryon Density Determinations
D 3He agree with the CBR
Depleted ?
N? lt 3 ?
(Steigman BBN)
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Third year SNLS Hubble Diagram (preliminary)
3/5 years of SNLS 250 distant SNe Ia
OM0.3, O?0
OM1.0, O?0
Reynald Pain told us about the French/Canadian
SNLS
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3-yr cosmological Constraints (Preliminary)
WMAP-3
SNe
7 measure of w
SNe
BAO
BAO
SNLSBAO (No flatness)
SNLS BAO simple WMAP Flat
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Three Year Yield 135 SNe, 50 SNe Ia, 25 SNe Ia
at zgt1 SNe Ia at zgt1 Appear Consistent with zlt0.1
(Adam Riess HST SN1a)
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Confirmation of the Dark Matter/Dark Energy Model
G R O U N D
S P A C E
Riess et al. 2004, 2007
Determining the nature of dark energy, its time
variability
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(Alex Kim SCP)
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From Peter Garnavitch, we learned more about SN1a

• SN1a may be better standard candles in the IR
  (less dust?)
• More SN1a in younger populations than
  ellipticals!
• Old galaxies may give fainter SN1a!
• Dark Energy is good for astrophysics!!!

These effects may be small, but are remarkable
and certainly call for more study. Systematics
such as these may give the ultimate limit for
SN1a as standard candles.
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Delayed Detonation Phenomenological Type Ia
Model White Dwarf ignites, burns slowly and
expands, then detonates.
deflagration (Sdef - parameter)
DDT (transition density rtr -
parameter)
detonation
ignition
Carbon-Oxygen
Silicon-group elements(28Si,)
Iron-group elements (56Ni,)
(Alexei Khokhlov SNIa)
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Detonation Phase of Explosion
Confirms one-dimensional DD model.
Qualitatively agrees with observations.
Asymmetries predicted.
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The power of weak lensing DM and DE
Weak lensing mass contours (HST) Extended
x-ray emission (XMM-Newton) Galaxy
number density (Subaru/CFHT) Galaxy
stellar mass (Subaru/CFHT)
R. Massey et al. (Nature 2007)
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Bullet cluster 1E0657-56
Doug Clowe, Marusa Bradac et al. (Astrophysical
Journal 2006)
1.5
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GLAST Large Area Telescope Overview Igor V.
Moskalenko HEPL - KIPAC Stanford
University Representing the GLAST Collaboration

International workshop on the interconnection
between particle and cosmology (PPC07) College
Station, TX, May 14 18, 2007
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• Win de Boer told us that already EGRET has the
  signal of DM! Including a ring made by the Canus
  Majoris Dwarf galaxy.
• Eiichiro Komatsu told us the same, including
  contributing much of the extra-galactic
  background.
• Thus we are really wanting to see what AMS and
  especially GLAST will give us -gt

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A.Morselli
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The Galaxy Shinning in High Energy Gammas from
the Annihilation of Dark Matter
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• Peskin told us we can get Wimp masses from LHC,
  but will probably need ILC to get the cross
  sections
• Tovey among others told us we need both LHC, and
  direct/indirect detection to prove we know what
  the DM is
• Gould told us what the dark matter is not (Machos)

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And finally, we heard that 1/3 of stars have cold
Neptune mass planets! Neither particle physics
nor cosmology yet!
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