Title: CMU
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2- 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
3Advantages 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
4Comparison 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
5Sensitivity to Dark Energy equation of
state
Volume element
Comoving distance
Huterer Turner
6Volume Element as a function of w
Dark Energy ? More volume at moderate redshift
7Cluster 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
8Instrument 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
9The optical system
10o
10New pn-CCD detector performance
0.28 keV
New pn-CCD
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12Ball RS300 Spacecraft
Stowed in 63? Taurus Fairing
On Orbit
13Observing 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
-
14Contiguous
Goal
DUO Wide
DUO Deep
Rosati, Borgani Norman ARAA 40, 539, 2002
15HEAO-1
DUO
10000
DUO
1000
XMM medium
100
ASCA LSS
XMM/Chandra deep
BeppoSAX
HELLAS2XMM
16Redshift distributions
2-10 keV X-ray flux versus R-band magnitude for
optically identified X-ray sources from Chandra
and ASCA X-ray surveys.
17One Square Degree of Deep Survey
18Discrimination of Clusters vs. Active Galactic
Nuclei
19Measurements of Dark Energy with DUO
WE
WM
w
WM
20P(k) Neutrinos
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