CMU

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• CMU
• Richard Griffiths - PI
• GSFC
• Robert Petre Deputy PI
• Keith Jahoda
• Richard Mushotzky
• Nicholas White
• MPE
• Guenther Hasinger Co PI
• Peter Predehl
• Hans Boehringer
• Peter Friedrich
• Lothar Struder
• Norbert Meidinger
• Eckhard Kendziorra
• Elmar Pfeffermann

Xavier Barcons IFC, Spain Lynn Cominsky
Sonoma State U. Patrick Henry U. Hawaii Abraham
Loeb Harvard U. Takamitsu Miyaji -
CMU BALL Steven Jordan William Purcell
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Advantages of X-ray Clusters
Can be well modeled X-rays are optically thin
thermal radiation from material nearly in
collisional equilibrium Not as simple as the
microwave background Simpler than supernovae,
galaxies or AGN Fewer projection effects with
X-ray selection X-rays are more peaked than
galaxy distribution Fewer foreground/background
objects Confining hot gas requires a real object
of high mass Close relation of X-ray observable
to cluster mass X-ray bright so seen to
cosmological distances Crucial 0 lt z lt 1
interval where universal expansion changed from
deceleration to acceleration
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Comparison of dark matter and x-ray cluster and
group distribution every bound system visible
in the numerical simulation is detected in the
x-ray band - bright regions are massive
clusters, dimmer regions groups,
X-ray emission in simulation
Dark matter simulation
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Sensitivity to Dark Energy equation of
state
Volume element
Comoving distance
Huterer Turner
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Volume Element as a function of w
Dark Energy ? More volume at moderate redshift
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Cluster Evolution and Cosmology
Borgani and Guzzo2001
X-ray properties of clusters trace mass

• The observables are the x-ray luminosity,
  temperature correlation function and their
  evolution with z
• x-ray properties directly connect to mass (Allen
  2002)

optical luminosity
X-ray luminosity
Mass
Mass
X-ray luminosity
kT
Mass temperature relation Horner et al 2001
kT
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Instrument HeritageABRIXAS and XMM

• DUO has a high degree of heritage
• 7 X-ray mirrors, focal length 1.6m
• Total field of view 3.3 sq. degs.
• Effective resolution 45 arcs.
• 7 PN-CCDs, 0.3 10 keV

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The optical system
10o
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New pn-CCD detector performance
0.28 keV
New pn-CCD
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Ball RS300 Spacecraft
Stowed in 63? Taurus Fairing
On Orbit
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Observing Strategy (eff. gt 60)

• DUO Deep SurveyDUO Deep Survey 150-DUO Wide
  Survey 6000 deg2
• hWithin SDSS Northern Galactic Cap
• h8000 clusters with M gt 2x1014 MO (kTgt3.5 keV)
  complete to z0.7
• hRedshifts already available
• DUO Deep Survey 176deg2
• h1800 clusters, about 200 at zgt1.0
• hSouthern Sky (ping-pong operation)
• hSynergy with large SZ-Surveys
• hOptical follow-up from VLT
• Operations Scan both regions in 2 years

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Contiguous
Goal
DUO Wide
DUO Deep
Rosati, Borgani Norman ARAA 40, 539, 2002
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HEAO-1
DUO
10000
DUO
1000
XMM medium
100
ASCA LSS
XMM/Chandra deep
BeppoSAX
HELLAS2XMM
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Redshift distributions
2-10 keV X-ray flux versus R-band magnitude for
optically identified X-ray sources from Chandra
and ASCA X-ray surveys.
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One Square Degree of Deep Survey
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Discrimination of Clusters vs. Active Galactic
Nuclei
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Measurements of Dark Energy with DUO
WE
WM
w
WM
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P(k) Neutrinos
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