Dark Universe Observatory Into the darkness peering…

Dark Universe Observatory

Into the darkness peering…


Into the darkness peering…CMURichard Griffiths - PI

GSFCRobert Petre – Deputy PI Keith Jahoda Richard Mushotzky Nicholas White

MPEGuenther Hasinger – Co PIPeter Predehl Hans BoehringerPeter Friedrich Lothar Struder Norbert Meidinger Eckhard Kendziorra Elmar Pfeffermann

Joseph Mohr – U. IllinoisZoltan Haiman – Columbia U.

Xavier Barcons – IFC, SpainLynn Cominsky – Sonoma State U.Patrick Henry – U. HawaiiAbraham Loeb – Harvard U.Takamitsu Miyaji - CMU

BALLSteven Jordan William Purcell



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 < z < 1 interval where universal expansion changed from deceleration to acceleration



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,

Dark matter simulation

X-ray emission insimulation


Into the darkness peering…Sensitivity to Dark Energy equation of state

Volume element

Comoving distance

Huterer & Turner


Into the darkness peering…Volume Element as a function of w

Dark Energy More volume at moderate redshift

Cluster Evolution and Cosmology• The observables are the x-ray

luminosity, temperature correlation function and their evolution with z

• x-ray properties directly

connect to mass (Allen 2002)

X-ray properties of clusters tracemass

Mass temperature relationHorner et al 2001

Borgani and Guzzo2001

X-r

ay lu

min

osit

y

Mass

Mas

s

kT

opti

cal l

umin

osit

y

X- r

ay lu

min

osit

y

kT


Into the darkness peering…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



The optical system

E [keV]

Tel

esco

pe A

EF

F [

cm-2]

(1 te

lesc

ope)

10o



New pn-CCD detector performance

ADU

Num

ber

of E

vent

s New pn-CCD

0.28 keV





Contamination Cover

Winston Cone

Spacecraft Bus

Single-Axis Driven Solar Array

Star Tracker

Telescope

Contamination Cover

Winston Cone

Spacecraft Bus

Single-Axis Driven Solar Array

Star Tracker

Telescope

On Orbit Stowed in 63 Taurus Fairing

Ball RS300 Spacecraft



Observing Strategy (eff. > 60%)• DUO Deep SurveyDUO Deep Survey: 150-DUO Wide Survey:

6000 deg2

Within SDSS Northern Galactic Cap

8000 clusters with M > 2x1014 MO (kT>3.5 keV) complete to z=0.7Redshifts already available

DUO Deep Survey: 176deg2

1800 clusters, about 200 at z>1.0Southern Sky (ping-pong operation)Synergy with large SZ-SurveysOptical follow-up from VLT

Operations: Scan both regions in 2 years



Rosati, Borgani & Norman ARAA 40, 539, 2002

Contiguous

Goal

DUO Deep

DUO Wide



XMMmedium

XMM/Chandradeep

HEAO-1

ASCALSS

10010

001000

0BeppoSAX

HELLAS2XMM

DUO

DUO



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.


Into the darkness peering…One Square Degree of Deep Survey



Discrimination of Clusters vs. Active Galactic Nuclei



Measurements of Dark Energy with DUO

w



P(k) Neutrinos



Dark Matter Hot Gas

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Dark Universe Observatory Into the darkness peering…

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