Radio galaxies in the Constellation X eraCambridge MA, July 8-11 2028Sebastian Heinz, UW-MadisonCollaborators:Marcus Brüggen, IU BremenPaul Nulsen, CfACon-X feedback panelFirst Generation Run...Heinz, Brüggen, Young, & Levesque 2006106 lightyearsMilky WaySimulated VLA movie of “Digital Cygnus A”:Simulated in a realistic galaxy cluster (from cosmo. sim.)1046 ergs s-1160 Myrs in 500 CPU daysResolution: 600 light yearsInterface: simulations/observations11Need to do 3d...“A simulation is only as good as its applicability to observations”Take a 3D simulation of thermal gasSimulate the spectrum emitted by the gas“Observe” it with an X-ray telescopeInterface: simulations/observations3minAs pointed out by Marcus and others:Clusters are not spherically symmetricAnd not hydrostaticI will argue:When simulating jet dynamics, crucial to include cluster dynamics and non-isotrpyNeed to do 3d...Features:Self consistent calculation of thermal plasma spectrum (APED)3D Input: density, temperature, velocity, metallicity, filling factorParameters: z, NH, vturb, texp, ...Telescopes supported: Chandra and Constellation X (full spectral response, simplified Gaussian PSF for now), others can be user-implementedArbitrary energy gridWritten in IDL, trivially parallelizedXIM: An X-ray visualization tool for numerical simulations of clusters3minAs pointed out by Marcus and others:Clusters are not spherically symmetricAnd not hydrostaticI will argue:When simulating jet dynamics, crucial to include cluster dynamics and non-isotrpyNeed to do 3d...Features:Self consistent calculation of thermal plasma spectrum (APED)3D Input: density, temperature, velocity, metallicity, filling factorParameters: z, NH, vturb, texp, ...Telescopes supported: Chandra and Constellation X (full spectral response, simplified Gaussian PSF for now), others can be user-implementedArbitrary energy grid (e.g., can easily make 3-color Chandra image)Written in IDL, trivially parallelizedXIM: An X-ray visualization tool for numerical simulations of clustersWill be made public shortlyBeta version available upon requestPlease send requests to heinzs@astro.wisc.edu3minAs pointed out by Marcus and others:Clusters are not spherically symmetricAnd not hydrostaticI will argue:When simulating jet dynamics, crucial to include cluster dynamics and non-isotrpyFirst Generation Run...Heinz, Brüggen, Young, & Levesque 2006Red: 0.3-2 keV, Green: 2-5 keV, Blue: 5-10 keV450 kpcThe Jet:W=1046 ergs s-1Run: 260 CPU daysOutburst: 3x107 yrsResolution: 170 pcThe neighborhoodS2 Cluster (Springel et al. 2001)1015M⦿ Clusterzstart=0.02The Chandra view8minInfinite S/NDynamic range optimized to show large scale imageNote: Clear temperature increase visibleClear cavities at later timesWave propagates faster when passed through cold frontRotation also visibleFirst Generation Run...Heinz, Brüggen, Young, & Levesque 2006The Jet:W=1046 ergs s-1Run: 260 CPU daysOutburst: 3x107 yrsResolution: 170 pcThe neighborhoodS2 Cluster (Springel et al. 2001)1015M⦿ Clusterzstart=0.02Red: 0.3-2 keV, Green: 2-5 keV, Blue: 5-10 keV450 kpcThe Chandra view9minClear outgoing shock signatureBut: also Turbulent wakeNote: The interior continues to excite ripples in the wake as jet sends out waves into cocoonSeries of outgoing sound waves visibleSome of the frothy structure in M87 might be due to this effect (partly induced by dentist drill)Need to do 3d...Two things Chandra lacksAreaSpectral resolution for extended sourcesConstellation X14minClear dynamic signature of expanding shellCon-X could do this for every pixelexquisit map of dyamical componentsThis could have also been done with XRS on SuzakuHighly encourage NGST (next generation Suzaku telscope)Need to do 3d...Two things Chandra lacksAreaSpectral resolution for extended sourcesEnter: Con-X< 15” angular resolution5 arcmin field of view> 10 x area3 Instruments, spanning 0.5-40 keVConstellation X14minClear dynamic signature of expanding shellCon-X could do this for every pixelexquisit map of dyamical componentsThis could have also been done with XRS on SuzakuHighly encourage NGST (next generation Suzaku telscope)Need to do 3d...Suzaku-like micro-calorimeterSpectral resolution: ΔE ~ 2.5 eV@6.4 keV: 2500 ~ 120km/s>100 x more area than gratingsIdeal for extended sources!Constellation X: XMS14minClear dynamic signature of expanding shellCon-X could do this for every pixelexquisit map of dyamical componentsThis could have also been done with XRS on SuzakuHighly encourage NGST (next generation Suzaku telscope)Need to do 3d...0.5-40 keV5m2 collecting area2-6 eV resolution (calorimeter)5” resolution (40” FOV)150 eV imager (7’ FOV)X-ray polarimeterX-ray Evolving Universe Spectroscopy “XEUS”14minClear dynamic signature of expanding shellCon-X could do this for every pixelexquisit map of dyamical componentsThis could have also been done with XRS on SuzakuHighly encourage NGST (next generation Suzaku telscope)Need to do 3d...Kinematics (down to few x 10 km/s)Shocks: few 100 km/sTurbulencePlasma diagnostics (precision spectroscopy)Polarimetry?Science capabilities:14minClear dynamic signature of expanding shellCon-X could do this for every pixelexquisit map of dyamical componentsThis could have also been done with XRS on SuzakuHighly encourage NGST (next generation Suzaku telscope)Need to do 3d...Science capabilities related to radio galaxies/clusters:kinematics (few x 10 km/s) in cold background (hard)turbulence (easy)plasma diagnostics (precision spectroscopy)14minClear dynamic signature of expanding shellCon-X could do this for every pixelexquisit map of dyamical componentsThis could have also been done with XRS on SuzakuHighly encourage NGST (next generation Suzaku telscope)Need to do 3d...250 ksecFe XXV & Fe XXVIHeinz et al. in preparationThe Con X view of Cygnus A14minClear dynamic signature of expanding shellCon-X could do this for every pixelexquisit map of dyamical componentsThis could have also been done with XRS on SuzakuHighly encourage NGST (next generation Suzaku telscope)Kinematics:Heinz et al. in preparationOther sources:Turbulent ICM ~ fee 100 km/sShock emission is more difficult to detect in low-Mach shocks:Look for AGN induced turbulenceDetailed plasma diagnostics: multi-temperature, shock jumpsDavid et al.SummarySimulators: request XIM beta now, download it when it becomes available ⇒ produce simulated Chandra and Con-X spectral cubesChandra simulations of Cyg A show shocks, cavities, wisps, froth,...Con-X will be a powerful tool to study radio galaxies and their environmentsCyg A and probably Cen A and a few other sources will clearly show the shock kinetmatically (velocity can just be read-off)Most clusters/groups will have to be analyzed in more detail, but will provide a rich array of plasma diagnostics.Make models now to help shape the future of Con X15min