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Hard X-ray Black Hole Surveys in Space and Time: EXIST Concept

Hard X-ray Black Hole Surveys in Space and Time: EXIST Concept. Josh Grindlay Harvard International Workshop High Energy Astrophysics in the Next Decade (Tokyo) June 21, 2006. Outline of talk. Key HEA and EXIST science questions Overview of EXIST as Black Hole Finder Probe (BHFP)

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Hard X-ray Black Hole Surveys in Space and Time: EXIST Concept

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  1. Hard X-ray Black Hole Surveys in Space and Time: EXIST Concept Josh Grindlay Harvard International Workshop High Energy Astrophysics in the Next Decade (Tokyo) June 21, 2006

  2. Outline of talk • Key HEA and EXIST science questions • Overview of EXIST as Black Hole Finder Probe (BHFP) • Current surveys to answer them: • X-ray: Chandra, XMM, Swift-XRT, Suzaku • Hard X-ray: INTEGRAL, Swift-BAT, Suzaku/HXD & BAT-slew • TeV: HESS, VERITAS • Upcoming surveys: • Agile, GLAST, LSST (approved) • MAXI, Lobster/eROSSITA, HXMT, Symbol-X (uncertain?) • “Ultimate” spectral-temporal HX survey: EXIST • Mission study for BHFP in Beyond Einstein Program…

  3. Key HEA Survey & EXIST Science (from the Galaxy to Pop III GRBs) • Nature/number of BHs vs. NSs, WDs in Galaxy • Blazar spectra @TeV vs. ~100keV: origin of EBL • Dormant AGN (tidal disruption by SMBHs) • SMBHs in every galaxy? BH masses from power spec. • Obscured AGN and origin of CXB • GRBs from Pop III stars: birth ofFirst BHs & probes of IGM

  4. High Energy Telescope HET (10-600keV) (6 x 3 coded aperture telescopes; 131o x 65o FoV) Low Energy Telescope LET (3-30 keV) (4 arrays of 7 x 1 coded aperture telescopes; 116o x 64o FoV) Overview of BHFP-EXIST Science and Design • Hard X-ray (~3-600 keV) all-sky imaging each orbit to measure: • Obscured AGN and accretion (BHs) vs. nuclear (stars) luminosity of universe • GRBs out to z ~20 and first stellar Black Holes ( ~5-20X Swift sensitivity) • Stellar Black Holes in Galaxy & IMBHs in Local Group & BHs as probes IMDC design Dec. 2004 e.g., EXIST measures Cen-A every orbit: characteristic time variability (QPOs) constrain BH mass • Mission Designparameters: • Extend ROSAT sens. (~5 x 10-13cgs) to 3-150 keV with 0.9-5’ resolution & ~10” positions • Two wide-field coded aperture telescopes: 10-600 keV (6m2 CZT) & 3-30 keV (1m2 Si) http://EXIST.gsfc.nasa.gov

  5. Expected EXIST Survey Sensitivity Continuum Narrow Line LET 3-30 keV; HET 10-600 keV 0.05mCrab = 5 x 10-13 cgs, (over any band Elow 2Elow) 5σ, 1yr, 20-40% duty cycle any source

  6. Hard X-ray Sky • Hard X-ray (10-600 keV) sky not yet surveyed to ROSAT sensitivity. EXIST would be ~20X more sensitive than Swift or INTEGRAL and cover full sky • EXIST will detect ≥3 x 104 sources, ≤10 positions, 3-600 keV spectra • EXIST would provide unique temporal survey: full sky imaging each orbit Previous Hard X-ray Sky HEAO-1, BeppoSAX ≤2010 Hard X-ray Sky Swift & INTEGRAL 2016(?) Hard X-ray Sky EXIST HXMT, eROSSITA?

  7. Survey BHs, NSs and WDs in Galaxy Integral and Swift/BAT discovery of hard, variable giants Wind-fed accretion onto NS or BH: Provides variable, high NH hard sources, with Lx >1036 erg/s as seen by Integral Simulations by J. Blondin Complements Swift discovery of transients & hard pulsars (15-150 keV) Lx >1036 erg/s& HESS (TeV) discovery of Be-binary PSRs Complements ChaMPlane Lx~1032 erg/s, high NH sources which are qLMXBs and CVs

  8. The Chandra Multiwavelength Plane Survey (ChaMPlane) Josh Grindlay, Ping Zhao, JaeSub Hong, Maureen van den Berg, Silas Laycock (Harvard, CfA) Distribution of ChaMPlane fields (●=ACIS-I, vs. o=ACIS-S) locations, exp. Times, & NH See Grindlay et al, Hong et al, Laycock et al, Zhao et al (2005, ApJ)

  9. Stellar mass BHs vs. CVs in Galactic Bulge? ChaMPlane survey and optical-IR followups: a mixture of magnetic CVs, NSs and BHs in SgrA* and Bulge… IR variable (red star in 0.5” Chandra circle) for a “Muno source” in H1 class: PossibleCH-Cam BH-LMXB? (Laycock et al 2006) Optical IDs with OGLE variables In “Stanek Window” : probable Wind-fed CVs, symbiotics (IPs?) (van den Berg et al 2006) Quantile diagram (see Hong et al 2004) for ~900 sources within 7’ of SgrA*: spectral classification & IDs (Hong et al 2006)

  10. Survey Stellar BHs & IMBHs in Local Group with EXIST • EXIST detects all bright stellar BHs in transients (Lx(>10 keV) ~1037-38 erg/s) throughout Galaxy, LMC/SMC and M31. Reveal population of obscured HX sources found with INTEGRAL/Swift: discrete sources at >20 keV • Isolated stellar BHs in Galaxy and IMBHs in Local Group accreting via Bondi-Hoyle (with ~10-4 efficiency) from GMCs nearly Compton thick • Faint BH transients in CentralGalactic Bulge?: BHs in nuclear cusp (cf. Alexander & Livio 04) detected if Lx(>10 keV) ~1035 erg/s CI Cam type outbursts (~1-2d?) of Bulge BH vs. WD binaries around SgrA* Chandra view of central Bulge (~ 2o x 1o)

  11. New Swift/BAT Slew Survey (BATSS) (being developed at CfA for Swift/BAT science & EXIST testing) • BAT slews ~60X/day between pointings; photon data could be sent down (1min/slew) for imaging all-sky survey (15-150 keV), ~1h/day fast timing gives: • GRBs & Long (High z) GRBs (30% more coverage) • New transients & pulsar monitoring (~70mCrab/orbit) • Stacked sky images for fainter transients (~20mCrab/d~90%sky) • New persistent sources • Test scanning for EXIST 70sec BAT slew image across CygX-1 (S/N~19) to a GRB (which was the z =6.3 event!)

  12. BATSS enables ~30% more GRBs & ~90% sky/day

  13. BATSS coverage & sensitivity vs. time(e.g. 10days in May, 2006…) ~30% increased detection probability for GRBs, transients, or steady sources is relatively constant w.r.t. GRB/transient duration. BUT only BATSS would provide photon timing; normal BAT data binned in 5min integ. Enables first all-sky PSR monitoring Survey since BATSE

  14. TeV Blazar surveys: constrain EBL & IRB(but only if constrain HX spectrum and variability) Ongoing HESS and (soon) VERITAS surveys discover new Blazars for comparison with X-ray & HX spectra New blazars detected by HESS at large z !H2356-309 (z=0.165), 1ES1101-232 (z=0.186) Reconstructing EBL (HESS collab., submitted to Nature)

  15. X- Blazar surveys • Agile & GLAST will discover flaring Blazars (~30MeV-30 GeV) • Swift/BAT, INTEGRAL give partial HX coverage • Swift/XRT, Suzaku, Chandra, XMM give partial X-ray coverage Need ~5-300 keV imaging & monitoring to constrain SSC Blazar SSC models Synch. IC Mkn 421 flares– 0.5h – 2d GLAST

  16. BlazarSpectralvariability: Extragalactic Background Light (EBL) & Stellar vs. Accretion Luminosity of Universe EBL: Hard x-ray (synchrotron) spectral breaks (~5-200keV) for Blazars at known redshift allow SSC -ray (~10 GeV - 10 TeV)spectralbreaksmeasured by GLASTand HESS/VERITAS to constrain origin of diffuse IR background Time-variability: spectral breaks required from simultaneous HX measurements. Wide-field HX imaging needed to match GLAST EXIST VERITAS GLAST SSC model for Mkn 501 (Coppi & Aharonian 1999) EXIST will provide the continuous HX spectral-monitoring to study Blazars and non-thermal AGN to constrain diffuse IR (~10-100μ) background from obscured AGN and thusnuclear vs. accretion luminosity of the universe Complements GRB science: star formation vs. redshift from LGRBs vs. z

  17. Dormant SMBHs revealed by Tidal disruption(and BH masses from AGN power spectra) Tidal disruption of stars spiraling into Dormant SMBHs with mass ~107 Mo: if 1% of Lacc in HX band, ~10-5 events/year/Mpc3 allow EXIST to see ~10-30 flares/yr out to ~200Mpc!(Grindlay 2004). HX spectral comp. “confirmed” withPL spectral decay of RX1242 Sub-giants with WD cores are gravitational wave LISA triggers. Artists conception of tidal disruption of star in RXJ1242-1119 detected with ROSAT (1991) and confirmed with Chandra (Komossa et al 2004). Possible soft (~5keV) prompt (~1d) burst detectable out to ~30 Mpc directly with EXIST (LET) and with MAXI or LOBSTER; LISA trigger Measure 106-7M SMBH content/evolution of nearby galaxies (understand BH-Bulge mass relation & BH-galaxy evolution!)

  18. EXIST survey SAX/PDS Swift HEAO Obscured AGN and origin of the CXB NGC1068 NGC6240 (Vignati et al 99) Chandra & XMM surveys find >40% unresolved CXB from obscured AGN EXIST will find >1-10 obscured AGN/square degree and obtain first all-sky measure of Seyfert 2 QSO 2 luminosity function and constrain obscuration vs. z for supermassive BHs. Provide required all-sky survey for rare (Type 2 QSOs) and Lx dependence of NH

  19. Birth of Stellar BHs at z~5-20 • “Long”-GRBs are from SNIb,c & likely due to stellar BH formation • Likely that first stars were ~100Mo and collapse to BHs GRBs • “Short”-GRBs from merging NSs in globulars (Grindlay et al 2006) suggests Short GRBs enhanced at z of globular cluster formation? EXIST detects GRBs to z~20 from PopIII BHs at re-ioniz. epoch suggested by WMAP. Photometric z from Lum-Epeak need response to E>300keV, And from Lum-Variability (Paczynski Relation) need large area det. X-ray flashes and high z GRBs need response to E~5 keV ~5sr instantaneous GRB coverage And increased sensivity: Rare (high z?) events; 3-5GRBs/d! Flux vs. detected Epeak for GRBs from z=1 (top +) to 10 (bottom +) for Epeak =30, 100, 300, 1000keV if emitted at z=1 vs. sensitivities (Band 2004).

  20. Highest z stellar universe uniquely from GRBs • Swift GRB at z = 6.3 shows high z universe is accessible • Broader energy band, higher sensitivity needed for z~20 PopIII • IR from space needed for z! • GRBs provide “back-light” for IR spectroscopy of IGM, gas, galactic structure back to re-ionization: EXIST + JWST? Record-setting z vs. time: GRBs are gaining fast!

  21. EXIST: Current Baseline Mission Design Concept (GSFC ISAL & IMDC runs Oct. & Dec. '04) High Energy Telescopes (HET: 10 – 600 keV) Zenith (Yaw) Thermal Radiator Orbit Normal (Pitch) Velocity (Roll) Low Energy Telescopes (LET: 3-30 keV) Solar Panels (fold-down) • Survey the hard X-ray sky 50x deeper than previous, • with 10 source positions (5) • Cover the 3 to 600 keV band with two telescope systems: • HET: 10 - 600 keV (5.6 m2 CZT) andLET: 3 - 30 keV (1.1 m2 Si)

  22. EXIST Mission Design Parameters • Free-Flyer (500km, i  5-7º, low bkgnd) • Zenith pointer - scanning & nodding for full sky coverage each orbit (95min) • 18 coded aperture HE telescopes (6m2 total area CZT pixel det.) • 28 coded aperture LE telescopes (1m2 total area Si drift det.) • Mass, power, telemetry: 9500kg, 3KW, 3Mbs • Delta IV launch (to i ~5o orbit) • Mission lifetime: 5 years Zenith Nod direction,┴ scan (+/-20o ea. ~10min) Orbit Normal Orbital scan direction (orbital velocity vector)

  23. Detector packaging: DCU, DCA, DM, Sub-Tel & HET Building a very large area CZT detector/telescope Detector Crystal Unit (DCU) Crystal (2x2 cm2) (with Interposer Board?) + 2 x 128 channel ASIC (with micro-via tech?) Detector Crystal Array (DCA) 2x2 DCUs (4x4 cm2) + FPGA Board HET 3x6 Sub-Tels (5.6 m2) Detector Module (DM) 7x7 DCAs (28x28 cm2) + MicroProcessor Board Sub-Tel Module 2x2 DMs (56x56 cm2); each of 18! Active & Passive shields

  24. Baseline Mission parameters: EXIST/HET & LET

  25. Advancing the Mission Design • The contiguous layout of HET sub-tel modules allows very efficient shield sharing and makes the overall instrument design simple and straightforward. • The current mission design already meets the mission parameters required for science goals. • However, the current layout introduces some unnecessary constraints on spacecraft design due to asymmetric packaging for launch. • Goal: Redistribute sub-tel modules symmetric for launch and increase total area in LET (and HET).

  26. New (General Dynamics) Design ConceptSymmetric, smaller solar panels & increased LET Area & FoV Zenith Orbit Normal HET Velocity LET Solar Panels Spacecraft Bus Stowed Delta IV (5m Fairing) On Orbit

  27. Side and Top Views of New Design

  28. Instrument Layout & FoV Comparison HET HET LET LET 131 112 154 160 64 64 65 65 Baseline Design HET: 5.6m2 (18 mods) LET: 1.1m2 (28 mods) New Configuration HET: 6.0m2 (19 mods) LET: 1.3m2 (32 mods) 

  29. Mission parameters for the new configuration

  30. Ensuring EXIST Imaging Performance • A wide dynamic range (>~103-4) to achieve high sensitivity impose challenges for coded-aperture imaging. • The main factor for limiting the performance in coded-aperture telescopes is noise caused by unknown systematics in the system. • These systematics include non-uniformity in the detectors such as detectorgaps, dead pixels, efficiency variations, background variations, etc. • EXIST’sscanning/nodding motion designed for surveying the sky is also a key to reduce the unknown systematics. • We demonstrate imaging performance of EXIST by a series of progressively realistic simulations. Swift/BAT slew imaging tests are in progress; and demonstration of EXIST detectors and imaging planned with ProtoEXISTballoon experiments.

  31. Example: Imaging noise caused by detector gaps (click for movies) Artifacts due to gaps start appearing at ~0.5 mm gap in the sky image generated by a simple correlationwithout any correction Scanning motion automatically averages out the coding noise without need for additional correction

  32. Simulated Scanning vs. Pointing with dead-pixels Assuming a fraction of unknown dead pixels in the detector, 1 day exposure of one sub-tel in EXIST HETs 5  detection limit with no other source or with a 1.5 Crab source Dynamic Range with a 1.5 Crab source

  33. Scanning vs. Pointing with a partially-coded source Assuming a partially coded source in the FoV & unknown 1 mm crystal gap, apply a CLEAN procedure for the partially coded source 5  detection limit with no other source or with a 1.5 Crab source Dynamic Range with a 1.5 Crab source

  34. BAT slew imaging provides on-orbit test And new Swift/BAT survey science… ~70sec scan detects CygX-1 @19 vs. 14 for pointing with BAT Noise reduced due to averaging effects of scan

  35. Prototyping EXIST • Balloon program to develop ProtoEXIST (Harvard, GSFC, Caltech, Stanford collaboration) • Phased development (ProtoEXIST1 ProtoEXIST2) (2.5mm 1.2mm pixel pitch & direct-bonded ASIC) • Demonstrate detectors & packaging, scanning imaging and (if ULDB?!) early EXIST survey science

  36. The current test board (poptart) allows testing 4 Detector Crystal Units (DCUs = crystal + IPB+ASIC) 1 DCU: 2cm x 2cm X 0.5 cm CZT Custom ASIC 64ch, 3 x 9mm pkg., ~150microW/channel

  37. Prototype Detector Performance Parasitic Capacitance of Input traces on Interposer board (IPB) (from simulations) FWHM measurements of a bare IPB using pulser Internal to ASIC

  38. Radiation Tests on prototype DCUs for ProtoEXIST1 ~4.7 keV FWHM from 120 keV (57Co) ~4.5 keV FWHM from 60 keV (241Am) We expect ~3 keV FWHM from the next batch (Aug ’06) of DCUs with improved (lower capac.) IPBs. (vs. ~1.5 keV for direct-bonded ASICs in ProtoEXIST2 and EXIST)

  39. Detector Crystal Arrays (DCAs) for ProtoEXIST1 Detector Crystal Unit (DCU) ASIC Top Socket Board Bottom FPGA Board FPGA (controls/reads out 8 ASICs on DCA)

  40. Assembled ProtoEXIST1 DCA (design complete; under fab.) Enable tiling of 4cm x 8cm CZT arrays with 0.4mm gaps

  41. Detector Module for ProtoEXIST1 (256cm2 close-tiled array of 8 DCAs) HV bias Detector Crystal Arrays (DCAs)

  42. Detector Module for ProtoEXIST1 Near gapless Packaging of 16cm x16cm CZT arrays EXIST sub-tels will have 56 cm x 56 cm CZT arrays.

  43. Summary • INTEGRAL and Swiftimaginghave revealed the rich HX sky (obscured binaries, AGN, high z GRBs…!) • Broad band (≥3 – 300 keV), large area and wide FoV are key. Unique all-sky imaging each orbit • HX surveys have enormous synergy with GeV-TeV (GLAST-VERITAS) studies of Blazars (and EBL) • Both obscured and dormant SMBHs best studied with wide-field very sensitive HX imager • Highest z universe uniquely measured via GRBs • EXIST under study for BHFP – could launch in ~2016 • See EXIST website (http://EXIST.gsfc.nasa.gov) for Study & team • ProtoEXIST1 balloon in 2008, ProtoEXIST2 in 2010…

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