BlankIntroConstellation X-ray Mission:Science and ProspectsConstellation X-ray Mission:Science and ProspectsPresented by Harvey Tananbaum (SAO) on behalf of theConstellation-X TeamHEAD-AAS!!!! New Orleans!! September 9, 2004Presented by Harvey Tananbaum (SAO) on behalf of theConstellation-X TeamHEAD-AAS!!!! New Orleans!! September 9, 2004CON-XMission parameters– Telescope area: 3 m2 at 1 keV 25-100 times XMM/Chandra for highresolution spectroscopy– Spectral resolving power: 300-1,500 2-3 times better than Astro-E2 at 6 keV– Band pass: 0.25 to 40 keV 100 times RXTE sensitivity at 40 keVUse X-ray spectroscopy to observe• Black holes: strong gravity & evolution• Dark Matter throughout the Universe• Dark Energy parameters• Production and recycling of the elementsEnable high resolution spectroscopy offaint X-ray source populationsAn X-ray VLTConstellation - XConstellation - XConstellation-X Mission OverviewConstellation-X Mission OverviewCON-XExploded View of Constellation-X ObservatoryExploded View of Constellation-X ObservatoryCON-XSXT Optical PathSXT Optical PathCON-XSXT Effective AreaSXT Effective AreaCON-X3.2m/1.6m x12m FL Configuration3.2m/1.6m x12m FL ConfigurationGrating Area(4 pl.)HXT (4)CalorimeterArea (2 pl.)0.8 m1.6 mSpacecraftAccommodationArea (2 pl.)2 Complete SXTs per launch• 2 sets of detectors req’d.3.2m OD x (4) 60º wedges forgratings(2) 1.6m Full Diameter Inner Tel.•0.3m ID12m Focal Length•Can be accommodated in19.1m fairing with fixed opticalbenchSXT raw glass weight ~850 kg•Should be OK for Delta-4HlaunchCON-XSXT Effective AreaSXT Effective AreaCON-X4m/2.4m with 25m FL 4m/2.4m with 25m FL ““BowtieBowtie”” configuration configurationGrating AreaHXT (4)CalorimeterArea1.2 m2 mSpacecraftAccommodationArea4m OD x (2) 90º wedges2.4m Full Diameter Optic•0.6m ID25m Focal Length•Requires extendable bench ormastSXT raw glass weight of 1085 kg•Should be OK for Delta 4Hlaunch, depending on weight ofextension hardwareCON-XSXT Effective AreaSXT Effective AreaCON-X4m/2m 1354m/2m 135 Wedge with 50m FL Configuration Wedge with 50m FL ConfigurationGrating Area (2 pl.)HXT (4)CalorimeterArea (2 pl.)1 m2 mSpacecraftAccommodationArea (2 pl.)4m OD x (2) 135º wedges2m IDGratings cover (2) 90º arcs50m Focal Length•Requires 2 spacecraftformation flyingSXT raw glass weight ~1304 kg•May stress launch capabilitiesof Delta 4H, depending on SXTstructural weight, andpropulsion requirementsooCON-X50.0 mOptics-craftDetector-craftX-axisZ-axisY-AxisOrbit configuration for 50m focal length separated s/cOrbit configuration for 50m focal length separated s/cCON-XSXT Effective AreaSXT Effective AreaCON-X 1. What happens close to a Black Hole?(thanks to Jon Miller, Chris Reynolds, Paul Nandra)2. What is Dark Energy?(thanks to Steve Allen, Richard Mushotzky)3. What is the Equation of State of Neutron Star? (thanks to Tod Strohmayer, Jean Cottam)This talk will concentrate on the Constellation-XThis talk will concentrate on the Constellation-XScience Goals in three Beyond Einstein Topics:Science Goals in three Beyond Einstein Topics:CON-XChandra Deep Field SouthChandra Deep Field SouthCDFSType2QSOR.Giacconi (AUI)CON-XType 2 Quasar at z = 3.7Type 2 Quasar at z = 3.7QuasarII/C-XConstellation-XChandraC.Norman (STScI)CON-XTheoretical‘image’ ofan accretiondisk.X-rays, (ComptonReflection andfluorescence)UVPrimarycontinuumopticalXMM-NewtonAccretion Disks and X-ray ReflectionAccretion Disks and X-ray ReflectionThe Iron fluorescence emission line is created when X-rays scatter and areabsorbed in dense matter, close to the event horizon of the black hole.CON-XMHD Simulations of Accretion Disk and Relativistic Iron Line EmissionMHD Simulations of Accretion Disk and Relativistic Iron Line EmissionC.Reynolds (U Md)CON-XBlack Hole FlareBlack Hole FlareC.Reynolds (U Md)CON-XGX 339-4GX 339-4J.Miller (CfA)CON-X• Con-X observations of broad iron line AGN– Variability of the broad iron line– Can “see” non-axisymmetric orbiting structures⇒ Direct measure of particle orbits close to BH– Line reverberation as flares sweep across disk⇒ Direct probe of photon orbits close to BH– Check for consistency with GR predictions (Kerr)– If OK, can measure BH masses and spins!– Otherwise, can constrain alternative space-time metric– Basic analysis technique does not rely on validity of GR or any other particulartheory (no template fitting needed to extract signal).• Comparison of AGN and Galactic Black Hole Binaries– Examine nature of gravity across 5-6 orders of magnitude in mass(using time-averaged line profiles)– GR predicts scale-independence… do we see that?• Con-X observations of neutron star absorption lines– Redshifts of NS emission lines are probe of the strong gravity– Constrains “RHS” of Field Equations, i.e., coupling of matter/fields tospacetime curvature (modulo e-o-s uncertainties)Con-X and Strong GravityCon-X and Strong GravityCON-XYou are hereΩmΩΛThe constraints from different techniqueson the mass content of the universe -notice that different techniques are“orthogonal” in this diagramNeed several precision techniques relatively freefrom systematic error or whose errors can bemeasured and quantifiedA major challenge to physics is that there is no “uniquenatural” candidate for dark matter and no physical theoryaccounts for the dark energy.Dark Energy and Dark MatterDark Energy and Dark MatterThe breakthrough may come fromincreased precision for each techniqueand disagreement between them!CON-XClusters of Galaxies are the largest objects in the Universeand the relative amounts of dark and baryonic matter(fgas = Ωb/Ωm) should be constant.This translates to a determination of the angulardiameter distance.A major strength of the method is that it gives preciseconstraints on Ωm as well as Dark Energy, therebybreaking a key degeneracy affecting other methods.The combination of fgas plus the CMB removes the needfor external priors.The Baryonic Fraction The Baryonic Fraction ““Standard CandleStandard Candle””CON-XChandra ResultsChandra ResultsSCDM Cosmology CDM CosmologyVS.Allen (IoA)CON-XCosmological ParametersCosmological ParametersS.Allen (IoA)CON-XDark Energy ParameterDark Energy ParameterSN1a SN1aClusters+CMBClusters(+BBNS + HST)S.Allen (IoA)CON-XAll the required quantities are directly measurablewith an X-ray image + spectrum and a S-Zmicrowave imageSensitivity to cosmological parameters due to Ωm,H0