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