Scaling Relations and Cosmology with EDGE and eROSITA

1
Scaling Relations and Cosmology with EDGE and
eROSITA

• Hans Böhringer, MPE Garching
• Importance of calibration of scaling relations
  for cosmology
• Status and future progress in scaling relations
• Prospects of EDGE and eROSITA

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Cosmological Constraints from Nearby Cluster
X-ray Luminosity Function
Cut-off Lx 0.03, 0.1, 0.25 x h-1 1044 erg/s
Perfect prediction of the Concordance
Cosmological Model for the Luminous Clusters from
the REFLEX Sample
Wm 0.23 0.35 (2s
without systematic uncertainties)
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Changing the M-L Normalisation
Change of the M-L normalization by factor 2
towards higher masses for given luminosity
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Constraints on Cosmological Models and Wm from
the REFLEX Cluster Survey
Combining the REFLEX cluster abundance with the
3dim power spectrum
Schuecker et al. 2002a,b
(curves are 1,2,3 s )
? DWm 0.34 -0.05 ( syst.
errors -0.05) 2s !
Universe with WL 0.7
and Wm 0.3
The large-scale distribution and cluster
abundance are consistent and can be combined to
improve the constraints !
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Constraints on Cosmological Models and Wm from
REFLEX Cluster Survey
ROSAT Schuecker et al. 2002a,b
(curves are 1,2,3s)
? Wm 0.34 -0.05 ( syst. errors
-0.05) 2s !
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Empirical LX Mass Relation
Lx
ext. HIFLUGS
HIFLUGS 63 clusters
mass
Reiprich Böhringer 2002
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M-T Relation Determined from XMM-Newton
Observations
Evrard et al. 1996
Borgani et al. 2004
gt 3.5 keV clusters
all clusters
The M-T relation determined from 10 relaxed
appearing gfalaxy clusters observed deepely with
XMM-Newton Arnaud et al. 2005
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Current Precision of Scaling Relationsfor nearby
clusters
Total matter density and gas mass density profiles
Comparison Arnaud et al. 05 and Vikhlinin et al.
06
diamonds Vikhlinin crosses Arnaud
M-T relation from 13 relaxed appearing galaxy
clusters observed deeply with Chandra Vikhlinin
et al. 2006 good agreement with the results
from Arnaud et al. 2005
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Accuracy of the Scaling Relation

• The scatter in the relation of regular, nearby
  clusters is less than 15, this is also the upper
  limit for the intrinsic scatter.
• This statistics has mostly been done for selected
  regular clusters. A systematic study for
  representative samples of clusters is in
  progress (REFLEX-DXL, XMM-LP, XMM-Medium Distant
  Clusters, HIFLUGCS).
• The mass has been derived in these studies
  using the spectroscopically determined
  temperatures Thus the two parameters have not
  been determined independently. Confirmation of
  the mass determination comes from the fact that
  gas mass fractions have bneen determined
  accurately.
• But see also results by E. Rasia on the problem
  of mass determination of multi-temperature
  plasma!

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Mass Temeprature Relation in Distant Clusters
Ettori et al. 2004
Maughan et al. 2006
The scatter in the relation is still very large
(- 30 50 in mass) - too large to make
significant distinctions between different
scaling models
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The Influence of w on Cosmic Evolution
Density fluctuation growth
open
L
w-0.6
w-0.2
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Evolution of the Cluster Mass Function
Differential comoving cluster abundance (gt
Masslimit) ster-1 dz0.1-1
? There are more distant clusters for small w !
See also Haiman et al. 2001
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Possible Constraints on w
Work by Majumdar Mohr 2003, 2004 - for
DUET, SPT, Planck Surveys (cluster population
out to 1.5)
Dw 4-5 20-40
10-20 4-6
cluster relations rel. unknown
P(k) P(k) follow-up
known (assuming 30 accuracy in mass
observing relations in follow-up studies)
A even higher accuracy of few percent is
necessary to probe for the time evolution of w
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Goals for Future Calibration Observations

• Get cluster temperatures for distant clusters to
  few percent accuracy similar to the present
  results for nearby clusters.
• Distinguish multi-temperature structure from
  single temperature structure

Edge cluster observation of a cluster at z1.4
Lx(0.5-2keV) 2 1043 erg/s 200ks obs DT
3 Dmetal. 10 50ks obs DT 10 Dmetal.
30
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Distinguishing Between 1- and 2- Temperature
Plasma
4 6 keV Plasma 1-temperature fit
2-temperature fit ( 5
Ms exposure) ?
sign. diff only with 5Ms
1 2 keV Plasma 1-temperature fit
2-temperature fit
(200 ks exp.) ?
sign. diff only with 50ks
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Constraints from 100K Cluster Survey
Time dependence of wx wx(z) w0 wa z
p(z) wx(z) r(z)
Results from the White Paper submitted to the
NASA/DOE Dark Energy Task Force Haiman, et al.,
2005, astro-ph/0507013
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P(k) and Baryonic Wiggles
Cluster Survey
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Constraints from Baryon Oscillations
100 000 clusters in survey required ! Schücker
2005, priv. comm.
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The eROSITA Survey
Main goal Study of Dark Matter and Dark Energy
using the Cluster abundance, the large scale
structure, the baryonic acoustic oscillations and
the cosmic evolution of clusters of galaxies with
a sample of 100 000 clusters
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The new Spectrum-X-Gamma Mission
Lobster
ART-XC
eROSITA

• Mission is approved on the Russian side. Launch
  planned on Soyus/Fregat from Baikonur in 2011.
• eROSITA funding secured, DLR project start
  planned for 1/2007
• Additional MPG funding for mirror and detector
  development

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New pn-CCD Chip Technology
Larger chips 384 x 384 pixels development
MPG is operating a dedicated semiconductor lab
for the development of novel detectors optimised
for high energy radiation. The new pn-CCD
detectors are significantly better, than those
successfully operated aboard XMM-Newton since
more than 6 years (energy resolution, CTI,
speed). 70 working CCDs are already available.
Larger chips currently being developed !
ROSITA Wafer in HLL on Cold Chuck Probe Station
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eROSITA

• 7 Mirror Systems
• ? 35 cm (ABRIXAS 16 cm)
• 54 gold-coated nickel-shells
• PSF lt 20 arcsec (goal 15 arcsec)
• Aeff 2400 cm2 (1 keV, on-axis)
• Grasp ?700 cm2 deg2 at 1 keV
• 7 individual cameras
• 256 256 pixel, 75µm
• 41 41 arcmin2 FoV
• framestore area

ABRIXAS
eROSITA
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Effective Area and Grasp
Effective area cm2 Grasp cm2
deg2
Grasp of 7 eROSITA telescopes is 3-4 x higher
than 3 XMM-Newton telescopes in the energy range
0.3-2 keV! At energies 5-15 keV, the Russian
ART-XC is taking over significantly.
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Schematic Exposure Map
Ca. 50
4 Years Surveyoptimised on extragalactic sky
(30000 deg2)significant survey of Galactic Plane
(10000 deg2)exposure rises towards the
poleseffectively ½ yr exposure in the poles of
the survey (2 x 200 deg2)
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Cluster Surveys
4y
eROSITA
1/2y
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Prospects of cluster surveys to various depth
x10
UCS
REFLEX2 (x100)