EMU/ eROSITA Complementarity for Galaxy Cluster Science (Cosmology)
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Transcript of EMU/ eROSITA Complementarity for Galaxy Cluster Science (Cosmology)
EMU/eROSITA Complementarity for Galaxy Cluster Science (Cosmology)
Thomas ReiprichArgelander Institute for AstronomyBonn Universityhttp://dark-energy.net
2012
2013
eROSITA TeamPI: Peter Predehl (MPE)Project Scientist: Andrea MerloniCo-Is: Hans Böhringer, Ulrich Briel, Hermann Brunner, Evgeniy Churazov, Michael Freyberg, Peter Friedrich, Günther Hasinger, Eckhard Kendziorra, Dieter Lutz, Josef Mohr, Norbert Meidinger, Kirpal Nandra, Mikhail Pavlinsky, Thomas Reiprich, Andrea Santangelo, Jürgen Schmitt, Axel Schwope, Matthias Steinmetz, Lothar Strüder, Rashid Sunyaev, Jörn WilmsSystem Engineer: Josef EderProduct Assurance: H. Bräuninger, M. HengmithElectronics Engineering: W. Bornemann, O. Hälker, S. Hermann, W. Kink, S. Müller, O. Hans, Z. Zhang, G. Plasoianu + Workshop Mechanical Engineering: H. Huber, Chr. Rohé, L. Tiedemann, R. Schreib, B. Mican, H. Eibl, A. Schneider, F. Huber, K. Lehmann, + WorkshopMirror System, PANTER: P. Friedrich, W. Burkert, M. Freyberg, B. Budau, , V. BurwitzCooling, Thermal Engineering: M. Fürmetz, E. Pfeffermann, A. BuronCCD-Camera: N. Meidinger, G. Schächner, J. Elbs, S. Ebermayer, A. v. KienlinAttitude: A. SchwopeCalibration, Analysis: G. Hartner, K. Dennerl, R. Andritschke, Chr. Tenzer Laboratory, PUMA, Tests: M. Vongehr, R. Gaida, K. Dittrich, Th. Burghart, T. Blasi, F. Schrey, K. HartmannGround Software, Simulation, Science: H. Brunner, P. Guglielmetti, G. Lamer, M. Mühlegger, J. Wilms, I. Kreykenbohm, C. Schmid, M. Brusa, A. Finoguenov, M. SalvatoMission Planning: J. Schmitt, J. RobradeScientific/Infrastructure Working Group Chairs: W. Becker, H. Böhringer, H. Brunner, K. Dennerl, M. Freyberg, F. Haberl, I. Kreykenbohm, J. Mohr, K. Nandra, T. Reiprich, J. Robrade, A. Santangelo, M. Sasaki, J. Schmitt, A. Schwope, J. Wilms
Institutes:MPE, Garching/DUniversität Erlangen-Nürnberg/DUniversät Tübingen/DUniversität Hamburg/DAstrophysikalisches Institut Potsdam/DMax-Planck-Institut für Astrophysik/DArgelander-Institut für Astronomie, Universität Bonn/DUniversitätssternwarte München/DSpace Research Institute IKI, Moscow/Ru
Industry:Media Lario/I Mirrors, MandrelsKayser-Threde/D Mirror StructuresCarl Zeiss/D ABRIXAS-MandrelsInvent/D Telescope StructurepnSensor/D CCDsEHP/B HeatpipesRUAG/A MechanismsHPS/D,P MLI+ many small companies
Instrument
Energy Range 0.5-10 keVEnergy Resolution 138 eV @ 6 keVDimensions 3,2m × 1,9m ØWeight 740 kg
Focal length 1,6 mField of View 1° Ø7 identical Mirror Modules54 nested Mirror Shells
Adapted from P. Predehl
Russian satellite
eROSITA
eROSITA StatusTelescope Structure
ready for integration ofsubsystems and components
Mirror Modules
FM-production running
FM1 (31 shells) in spec.FM2 (15 shells) in spec.
15 arcsec HEW, on-axis
Provided by P. Predehl
pnCCD-Camera
pnCCD Module working since 2010,in spec
size: 384 × 384 pixels = 28.8 × 28.8 mm2
cycle time: 50msecenergy resolution138eV @ 6 keV
Provided by P. Predehl
Data hyper-cube
Simulations
Pointing ScanOff-axis blurring of a Wolter-I telescope PSF has to be averaged over the FoV (1°)15 arcsec on-axis 28 arcsec averaged
Provided by P. Predehl
Historical Development
Spectrum-XGJet-X, SODART, etc.
ROSAT1990-1998
First X-ray all-sky surveywith an imaging telescope
ABRIXAS
1999
Bundle of 7 small telescopesTo extend the all-sky surveytowards higher energies
ROSITA2002
ABRIXAS science on the International Space Station
Negotiations between Roskosmos and ESAon a "new" Spectrum-XG mission (2005)
MoU between Roskosmos and DLR (2007)
eROSITA
Spektr-RGLaunch: 2013
Dark Energy105 Clusters of Galaxies
DUO2004
Provided by P. Predehl
eROSITA
Mr. Putin gets informedabout Dark Energy...
Provided by P. Predehl
From G. Hasinger.
ROSAT: 1 all-sky surveyeROSITA: 8 all-sky surveys
Comparison with other Surveys
Provided by P. Predehl
HIFLUGCS
Norris et al. (2011)
Expected eROSITA Exposure Map
Provided by J. Robrade
Galactic coordinates
seconds
Germany???Russia???
EMU Sky Coverage
Norris et al. (2011)
Provided by J. Robradeseconds
HIFLUGCS
Galactic coordinates
RASS ¼ keV Map
Data from S. Snowden.
eROSITA: more sensitive, better PSF, larger energy band.
NH Distribution
LAB survey, from P. Kalberla.
Main Science Driver for eROSITA: Cosmological Constraints from ~100,000 Galaxy Clusters
(First “Stage IV” Dark Energy Experiment World-Wide, Albrecht et al. 2006)
Pillepich, Porciani, Reiprich, to be subm.
Limiting Luminosity and Mass
Pillepich, Porciani, Reiprich, to be s.
Pillepich, Porciani, Reiprich,to be subm.~93,000 clusters
Possible Role of EMU
• EMU will likely detect 10s of thousands of clusters (Melanie’s talk, Norris et al. 2011). Combination with X-ray data (from eROSITA) will allow us to study cluster physics in detail and with great statistics. But how can EMU be useful for eROSITA cluster cosmology?
Dependence of Total Number of Detected Clusters on LX−M Relation
Patrick Lieberz, Bachelor Thesis (2011)
~50% more clusters
LX−M Relations
z = 0.5
Patrick Lieberz
Vikhlinin et al. (2009)Mantz et al. (2010)
LX
M
Higher LX
for given M
Dependence of LX−T Relation on Presence of Central Radio Soure (CRS) and on Dynamical
State
CRS slope = 3.2NCRS slope = 2.5
SCC (proxy for relaxed) slope = 3.3NCC (proxy for merger) slope = 2.4
Mittal et al. (2011), based on complete HIFLUGCS sample.
Possible Role of EMU
• Classifying into CRS and NCRS clusters could be useful for a better differentiation of applicable scaling relations, resulting in more robust cosmological constraints. EMU will be able to detect CRS for many eROSITA clusters.
• Same applies for relaxed and disturbed clusters. Radio halos, typical radio relics, and NATs/WATs reside almost exclusively in disturbed clusters, and EMU will find ‘em.
van
Wee
ren
et a
l. (2
010)
Cassano (2011)
Norris et al. (2011)~EMU-Wide,C. Ferrari
Follow-up ObservationsBottleneck for Some Studies
Needs for follow-up:• Enabling studies of cosmology and cluster physics: Redshift: phot-z + spec-z; mass estimation: weak lensing + velocity disersions • Evolution of AGN population (~3 million will be detected)
Redshift: (phot-z +) spec-z• Galactic sources
Follow-up context for eROSITA (List not complete!)• Shallow Multiband OIR Surveys 2MASS, PanSTARRS, SDSS• Deep Multiband OIR Surveys VISTA, DES• Optical Spectroscopic Surveys SDSS, BOSS• Proposed Optical Spec. Surveys 4MOST, BigBOSS, SPIDERS, WEAVE, Euclid• Future OIR Imaging Surveys LSST, Euclid
Radio surveys• ASKAP/EMU, WODAN, LOFAR
Sub-/mm• Planck, SPT, ACT
Adapted from P. Predehl
From A. Pillepich