Cosmology with the eROSITA all-sky survey of galaxy clusters
Cosmology with the eROSITA all-sky survey of galaxy clusters
Cosmology with the eROSITA all-sky survey of galaxy clusters
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The eRosita X-ray <strong>all</strong>-<strong>sky</strong> <strong>survey</strong>,<strong>galaxy</strong> <strong>clusters</strong> & cosmologyNicolas Clerc – MPE (Garching) for <strong>the</strong> eRosita team “Synergis*c science <strong>with</strong> Euclid and <strong>the</strong> Square Kilometre Array” Oxford – Sep., 17 th 2013
The eRosita telescopes• 7 idenFcal X-‐ray telescopes (Wolter-‐I, pn-‐CCD) • FoV = 0.8 deg 2 • PSF = 15” • A eff = 1300 cm 2 @1keV • Energy range 0.5-‐10 keV • Energy resoluFon 20-‐50 • 740 kg • 3.2m x 1.9m N. Clerc – Oxford – 17 Sept. 2013
eRosita collaborationPI: Peter Predehl; PS: A. Merloni (MPE)Core Institutes (DLR funding):MPE, Garching/DUniversität Erlangen-Nürnberg/DIAAT (Universät Tübingen)/DSB (Universität Hamburg)/DAstrophysikalisches Institut Potsdam/DAssociated Institutes:MPA, Garching/DIKI, Moscow/RuUSM (Universität München)/DAIA (Universität Bonn)/DIndustry:Media Lario/I Mirrors, MandrelsKayser-Threde/D Mirror StructuresCarl Zeiss/D ABRIXAS-MandrelsInvent/D Telescope StructurepnSensor/D CCDsIberEspacio/E HeatpipesRUAG/A MechanismsHPS/D,P MLI+ many sm<strong>all</strong> companiesMPE: Scientific Lead Institute, Project ManagmentInstrument Design, Manufacturing, Integration & TestData Handling & Processing, Archive etc.N. Clerc – Oxford – 17 Sept. 2013
Historical developmentSpectrum-‐XG Jet-‐X, SODART, etc. First X-‐ray <strong>all</strong>-‐<strong>sky</strong> <strong>survey</strong> <strong>with</strong> an imaging telescope ROSAT 1990-‐1998 Nego*a*ons between Roskosmos and ESA on a "new" Spectrum-‐XG mission (2005) MoU between Roskosmos and DLR (2007) „Detailed Agreement“ (2009) Bundle <strong>of</strong> 7 sm<strong>all</strong> telescopes To extend <strong>the</strong> <strong>all</strong>-‐<strong>sky</strong> <strong>survey</strong> towards higher energies ABRIXAS 1999 <strong>eROSITA</strong> ABRIXAS science on <strong>the</strong> Interna*onal Space Sta*on ROSITA 2002 DUO2004Dark Energy 10 5 Clusters <strong>of</strong> Galaxies (from P. Predehl, MPE) N. Clerc – Oxford – 17 Sept. 2013
eRosita on SRGART-XCIKI<strong>eROSITA</strong>MPENavigatorNPO LavochkinCredit NASA / WMAP Science Team • Launch to L2 [WMAP, Herschel, Planck + Gaia, JWST…] from Baikonour <strong>with</strong> Zenit-‐Fregat (Q4 2014) • 3 months flight to L2: verificaFon & calibraFon phases • 4 years <strong>all</strong>-‐<strong>sky</strong> <strong>survey</strong> (8 × ½ yr) • 3.5 years pointed observaFons (~20% GTO, 1 AO per year) • Proprietary data shared 50/50 MPE/IKI • German half: proprietary period max. 2 yrs • Periodic release <strong>of</strong> German <strong>all</strong>-‐<strong>sky</strong> data
eRosita effective area and graspEffective Area!Grasp Merloni et al. 2012 “eRosita science book” N. Clerc – Oxford – 17 Sept. 2013
eRosita PSF• 15” on-‐axis HEW (@ 1.5 keV) è 28” <strong>survey</strong>-averagedN. Clerc – Oxford – 17 Sept. 2013PANTER FM2 focal plane measurements @ 1.49 keV (image NC, Panter-‐MPE)
StatusStatus • Telescope Structure: PFM Complete • Mirrors: Qualified, ~95% <strong>of</strong> <strong>all</strong> shells integrated • Cameras: Qualified (incl. p-‐radiaFon), in spec, CCDs 100%, FM Cooling System: PFM complete • X-‐ray Baffles, Electron Deflector, Filterwheels etc: qualified, in manuf. • FM-‐Electronics: Behind schedule • QualificaFon tests <strong>of</strong> completer telescope completed (Jan 2013) • Delivery and test <strong>of</strong> Technological Model to Lavochkin (March 2013) • FM1, FM2, FM3, FM8 Mirror modules completed and tested; FM5 tests underway Next steps • FM4-‐7 Mirror Modules tests and integraFon Jun-‐Dec 2013 • FM electronics producFon and tests F<strong>all</strong> 2013 -‐ 2014 • Delivery to Lavochkin April/May 2014 • SRG Launch Q4 2014 (TBC)
eRosita <strong>all</strong>-<strong>sky</strong> <strong>survey</strong> (eRASS=8*6 mths)Simulated <strong>eROSITA</strong> field point-sources (no cluster) AnimaQon: 1 frame=6 months NC, C.Schmid, H.Brunner… (circle ∅=3 deg) N. Clerc – Oxford – 17 Sept. 2013
eRosita <strong>all</strong>-<strong>sky</strong> <strong>survey</strong> performance<strong>eROSITA</strong> ROSAT EffecFve Area @ 1keV 2000 cm 2 350cm 2 Angular ResoluFon (<strong>survey</strong>) 30 arcsec 60 arcsec Spectral ResoluFon ~100eV ~400eV Field <strong>of</strong> View 1° Ø 2° Ø Survey DuraFon 4 years ½ year Point sources Extended sources N. Clerc – Oxford – 17 Sept. 2013
eRosita <strong>all</strong>-<strong>sky</strong> <strong>survey</strong> performance<strong>eROSITA</strong> ROSAT EffecFve Area @ 1keV 2000 cm 2 350cm 2 Angular ResoluFon (<strong>survey</strong>) 30 arcsec 60 arcsec Spectral ResoluFon ~100eV ~400eV Field <strong>of</strong> View 1° Ø 2° Ø Survey DuraFon 4 years ½ year Point sources Extended sources Point source sensiFvity: ~30 Fmes deeper than ROSAT (sow band 0.5-‐2 keV) ~100 Fmes bexer than HEAO/RXTE (hard band 2-‐10 keV)
Data rights and Policies• German <strong>eROSITA</strong> data made public awer 2 yr proprietary period • Periodic data releases envisaged (e.g. 6, 18, 48 months) • Proprietary data via German <strong>eROSITA</strong> ConsorFum • Projects/Papers regulated by Working Groups • Individual External CollaboraFons • Group External CollaboraFons (negoFaFons/discussions underway <strong>with</strong> DES, CAASTRO, HSC) Science Working Groups:Clusters and <strong>Cosmology</strong>AGN, BlazarsNormal GalaxiesCompact objectsDiffuse emission, SNRStars, Solar SystemInfrastructure Working Groups:Time Domain AstrophysicsData analysis, source extraction, catalogsMulti-wavelength follow-upCalibrationBackground
The X-ray (extragalactic) universeDiffuse X-‐ray emizng gas traces <strong>the</strong> massive knots <strong>of</strong> <strong>the</strong> cosmic web (Clusters) Surveys <strong>of</strong> highly biasedpopulations (Clusters and QSOs)over large volumes can be done atvery high completeness levels!Point sources (Quasars) signpost <strong>the</strong> growth <strong>of</strong> black holes N. Clerc – Oxford – 17 Sept. 2013
Galaxy cluster cosmologyESA/PlanckExpansionGravitationMergers/Collisions(+baryonic physics)Simulation Horizonz>1000• Clusters <strong>of</strong> galaxies = tail <strong>of</strong> <strong>the</strong> halo mass distribuFon • ExponenFal sensiFvity to cosmological parameters • X-‐ray emission from baryons in <strong>the</strong> intra-‐cluster medium • Current cosmo constraints from ROSAT samples + calibraFon (Vikhlinin+09, ~ 100 objects) • Near-‐term constraints <strong>with</strong> XMM (sm<strong>all</strong> deep fields, few 100s low-‐mass objects, e.g. XMM-‐XXL, Pierre+11) N. Clerc – Oxford – 17 Sept. 2013
Galaxy <strong>clusters</strong> in <strong>the</strong> eRASS~100,000 <strong>galaxy</strong> <strong>clusters</strong> total Peak at z ~ 0.3 , M 500 ~ 10 14 M sol X-‐ray data alone will give: • Sky posiFon • Flux ↔ L X , z,… • Spectrum ↔ T X , z, abundances… • Morphology ↔ R 500 , z, M gas , substruct… UlFmately related to <strong>the</strong> (M, z) and 3-‐D (e.g. Reiprich & Böhringer+02 w/ROSAT ; Clerc+12 w/XMM) è Not simply “a deeper ROSAT <strong>survey</strong>”!
Main cosmological probesCluster counts: dn/dz/dM – dn/dz/dT/dL – dn/dz/d(X observable) – dn/dz/d(X)/d(o<strong>the</strong>r) Clerc+12 Planck 2013 SZ Vikhlinin+09
Main cosmological probesCluster 3D distribuFons – P(k,z,M,…) [Schuecker+03, Balaguera-‐Antolinez+11] and bias evoluFon – BAO/Alcock-‐Paczin<strong>sky</strong> – RSD (?) [e.g. Valageas & Clerc 12] – Cluster environment & super<strong>clusters</strong> [e.g. Chon+13] Guzzo+ 2009 N. Clerc – Oxford – 17 Sept. 2013
A DE Stage IV experiment-‐ X-ray (<strong>eROSITA</strong>) selection- Redshift determination- Mass calibration (dedicated follow up)- Cluster Mass function vs. z- Cluster Power Spectrum vs. z(photo-z)(spec-z)Merloni et al. 2012Pillepich et al. 2012
Optical/NIR <strong>survey</strong>sIKI(R) D/R split MPE(D) Image A. Nishizawa (IPMU),Andrea Merloni (MPE)X-‐ray alone not sufficient à Deep, mulF-‐filter to confirm <strong>galaxy</strong> overdens. / red-‐sequence / photo-‐z
Follow-up: spectroscopy• SDSS-‐IV (North) à SPIDERS (PI Merloni) – 2014-‐2019: early follow-‐up over a ~9000 deg2 area in <strong>the</strong> NGC: reach >80% completeness for eRASS:4, ~100,000 unique X-‐ray selected spectra • VISTA/4MOST (South) – 2019-‐2024: Complete, systemaFc follow-‐up <strong>of</strong> both Clusters and AGN from eRosita: reach >80% completeness for eRASS:8 – Approved awer Conceptual Design Phase, will start Phase B in 2014 Expected r AB magnitude distribuQon <strong>of</strong> 0.5-‐2 keV selected AGN in <strong>eROSITA</strong> <strong>survey</strong>s
SKA (and pathfdrs) & <strong>galaxy</strong> <strong>clusters</strong>• Radio-‐halo detected <strong>clusters</strong> vs. X-ray detected <strong>clusters</strong> • Dynamical state classificaFon and X-ray scaling relaFons (e.g. H.Roefgering’s talk) • AGN past acFvity (radio bubbles, etc.) è Feedback in <strong>the</strong> ICM • Relics (past merging acFvity, shocks) • Non-‐<strong>the</strong>rmal X-‐ray emission quanFfiable (CRS=Central Radio Source) Mifal+11 Wing&Blanton 11 • Bended radio tails (distant <strong>clusters</strong> searches) [e.g. Blanton+03] • Cross-‐correlaFons radio-‐gal/X-‐ray (extended/point-‐sources/background) Van Weeren et al. N. Clerc – Oxford – 17 Sept. 2013
Euclid & eRosita <strong>galaxy</strong> <strong>clusters</strong> (1/2)• Combined opFcal/X-‐ray searches for GCl up to z>~1 – Currently: RASS⊗SDSS (z
Euclid & eRosita <strong>galaxy</strong> <strong>clusters</strong> (2/2)• Improved mass calibraFon through WL+X-‐ray(+SZ Planck) – WL DM density pr<strong>of</strong>iles – X-‐ray gas density pr<strong>of</strong>iles+3-‐d structure – Tests <strong>of</strong> CDM <strong>with</strong> substructure – Stacking <strong>of</strong> X-‐ray data at <strong>the</strong> posiFon <strong>of</strong> Euclid GC • Galaxy alignments in <strong>clusters</strong> vs. field (“γ grav ”) • eRosita deep field/Euclid deep field: obvious synergy (e.g. distant <strong>clusters</strong> searches/characterizaFon) • eRosita pointed phase follow-‐up start ~2019, duraFon 3.5 yrs: 15” HEW, ➚depth N. Clerc – Oxford – 17 Sept. 2013
Summary• eRosita: an X-‐ray <strong>all</strong>-‐<strong>sky</strong> <strong>survey</strong> coming soon! – 10 5 <strong>clusters</strong> up to z>~1 – DE <strong>Cosmology</strong> and LSS studies – Cluster physics & mulF-‐λ synergies • 3 millions X-‐ray AGN: large, low-‐biased sample – Physics (<strong>galaxy</strong> evol, BH growth…) and cosmology (LSS,…) – Obvious synergies <strong>with</strong> SKA and Euclid! • ExciFng galacFc science • <strong>eROSITA</strong> Science Book: arXiv:1209.3114 • To be updated <strong>with</strong> synergy studies/forecasts! N. Clerc – Oxford – 17 Sept. 2013
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