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The keV – TeV Connection eRosita, Simbol X and the others… X-ray Observatories in the CTA era

The keV – TeV Connection eRosita, Simbol X and the others… X-ray Observatories in the CTA era. Andrea Santangelo IAAT. Outline of the talk. Only some of planned/designed/studied X-ray Observatories will be introduced….

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The keV – TeV Connection eRosita, Simbol X and the others… X-ray Observatories in the CTA era

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  1. The keV – TeV ConnectioneRosita, Simbol X and the others… X-ray Observatories in the CTA era Andrea Santangelo IAAT Towards A CTA FP7 Design Study

  2. Outline of the talk Only some of planned/designed/studied X-ray Observatories will be introduced… • The KeV – TeV Connection: a few reasons of the “science case” (not exhaustive) • A golden age for X-ray astronomy • eRosita • Simbol X • The Others (MIRAX, HXMT, NEXT, EXIST…) (not exhaustive) • Considerations Towards A CTA FP7 Design Study

  3. X-ray observation tracing the synchrotron emission of relativistic electrons are well suited to the identification of VHE Gamma Ray emitters Identification of Sources (Funk et al., astro-ph/0609586) Association is certainly spatial/morphology coincidence… • Hess ~2’(Aharonian et al., 2006) • ASCA AX J1813-178, highly absorbed, Hard (~1.8), extended • INTEGRAL IGRJ18135-1751 (Ubertini et al., 2006), softer than ASCA • Swift-XRT (Landi 2006), hard source, highly absorbed • VLA 20 and 90 cm young (~ 1ky) shell like SNR2.5’ diameter (G12.82-0.02) coincident with HESS (Brogan 2005) • XMM spectral and morphological studies, (Funk et al. 2006),compact core, extended tail, non thermal, highly absorbed Towards A CTA FP7 Design Study

  4. Identification of Sources (2) (Funk et al., astro-ph/0611646) It’s the positional and morphological coincidence that allows identification XMM-Newton map around HESS J1813-178 • Compact X- ray core • Extended with a hard tail toward North-East • Embedded in the radio shell type SNR G12.82-0.02 • Hard Spectrum Pulsar Wind Nebula, Composite SNR, even if …. Towards A CTA FP7 Design Study

  5. HESS 1303-631, HESS J1614-518, HESS 1702-420, HESS J1708-410… Aharonian et al. -HEGRA collab.-, 2005 • Prototype of Unidentified sources discovered by HESS • Spectrum is a power law (~1.9), extended • Gamma Ray Excess from Cygnus, Milagro (Abdo et al., 2006) • Radio Emission (Peredes 2006 • X-ray studies, (Butt 2006, Mukherjee 2006) • A deep, 50 ksec XMM Analysis is on going… (Horns et al., submitted) Search for faint extended emission, high sensitivity for low surface brightness Identification of sources (3) It’s not so easy, the case of Unidentified sourcesmay be very faint Towards A CTA FP7 Design Study

  6. A multimavelength coherent picture (Aharonian et al., astro-ph/0611813) Identification, that is understanding, implies that a coherent multiwavelength scenario must emerge See also RX J0852.0-4622 • Contours are from ASCA (1-3 keV band) • Correlation is amazing • A single electron population generates both the X (Sync.) and the Gamma (IC) radiation • Particle acceleration up to 100 TeV is required • Model interpretation is not so easy (Lemoine et al., 2006) HESS map of RX J1713.7-3946 Towards A CTA FP7 Design Study

  7. Spatially resolved spectral capability at X-rays is key A key example: synchrotron cooling Towards A CTA FP7 Design Study

  8. H.E.S.S. 0.25-30 TeV 20 pc X-rays TeV • Middle age PWN (21 kyears) • The Pulsar powers an asymmetric synchrotron nebula, arcmin size in X-rays • The VHE emitting region is wider • shorter range of X-rays electrons due to synchrotron cooling Gensler et al., 2003 XMM 2-10 keV Malizia et al., A&A 2006 HESS J1825-137 Aharonian et al., A&A 2006 Towards A CTA FP7 Design Study

  9. It coincides with the X-ray emission features observed with ROSAT and ASCA (2-10 keV) Map below PSR B0833−45 Vela pulsar • Middleage PWN (11 kyears) • The Pulsar powers an asymmetric synchrotron nebula, observed in X-rays • The VHE emitting region is slightly wider • Leptonic or Hadronic production ? (Horns et al., 2006) Vela X Aharonian et al., 448 A&A, 2006 ROSAT contours no emission from Vela pulsar detected Towards A CTA FP7 Design Study

  10. Horns, D. et al. 2006, A&A Hadronic interpretation Towards A CTA FP7 Design Study

  11. Spatially resolved spectral capability at Hard X-rays is essential Towards A CTA FP7 Design Study

  12. W. Hermsen, 2006 Albert et al., 2006 Timing…LSI +61 303, LS 5039 Towards A CTA FP7 Design Study

  13. An “amazing” effort… Towards A CTA FP7 Design Study

  14. High-Energy Observatories 2004-2020 SRG/ROSITA/Lobster (SIMBOL-X) MIRAX (XEUS) (NeXT) HMXT GLAST Agile Suzaku Con-X Swift Chandra XMM-Newton Integral 2004 2004 2006 2006 2014 2014 2016 2016 2010 2010 2012 2012 2018 2018 2008 2008 2020 2020 Brasil China Europe JAXA ESA Towards A CTA FP7 Design Study NASA

  15. Spectrum X-Gamma • eRosita (X-ray mirror Telescope) Germany • LOBSTER(UK) wide field monitor • ART(IKI, Russia) Hard X-ray concentrator • GRB detector (IKI, Russia) eROSITA Lobster ART-XC Sun direction 30 Rotation axis Platform Towards A CTA FP7 Design Study

  16. eRosita: history ROSAT (1990 – 1998) ~200,000 new X-ray sources Diffuse emission on all scales ABRIXAS (1999) 7 Wolter-Teles., 27 shells each sharing 1 pn-CCD Camera Rosita ISS (2000) 7 Wolter-Teles., 27 shells 7 pn-CCD Camera • Extension of RASS towards 10 keV • Detection of obscured AGN Towards A CTA FP7 Design Study

  17. N E Rosita evolved into DUO (2004) Proposal to NASA (SMEX, not accepted) Wide Survey 6,000 deg2 (SDSS)~ 8,000 clusters of galaxies < z~ 0.7 Deep Survey 176 deg2~ 1,800 clusters of galaxies < z ~ 1.2 Cosmology comes in: Luminous baryons give information about the distribution of Dark Matter, DUO-Simulation 1 deg2 Constrain the equation of state of the dark energy and the dark matter density, and measure how they evolve with time in the local Universe, using clusters of galaxies as mass tracers Towards A CTA FP7 Design Study

  18. eRosita on SRG (2005) • 7 Mirror Systems •  35 cm (ABRIXAS 16 cm) • 54 gold-coated nickel-shells • PSF < 20 arcsec (goal 15 arcsec) • Aeff ~ 2400 cm2 (1 keV, on-axis) • Grasp 700 cm2 deg2 at 1 keV • 7 individual cameras • 256 × 256 pixel, 75µm • 41 × 41 arcmin2 FoV • framestore area • energy range 0.2-12.0 keV • energy resolution 130 eV at 6 keV ABRIXAS eROSITA Funds already in the DLR budget, expected by June MOU will be signed soon, Launch date, late 2010-2011. Towards A CTA FP7 Design Study

  19. eRosita: science goals • Study the equation of state of DE with 100,000 Clusters • Numbers of Clusters as a function of redshift • Cluster power spectrum on large scales: p(k) • Baryonic acoustic oscillation in the cluster distribution (BAO) • Detect 1 Million Active Black Holes, many hiding behind obscuring gas and dust clouds • All sky survey is a factor of 50 deeper than ROSAT (0.5-2 keV) • A factor of 100 deeper than HEAO-1 (2-10 keV) • Study coeval evolution of Black Holes and galaxies (BAO) • Study of accretion and acceleration processes in a large variety of galactic sources • X-ray Binaries, Isolated Neutron Star, Cataclysmic variables • Coronal Stars, embedded protostars, interstellar medium • Supernova Remnants Towards A CTA FP7 Design Study

  20. Effective Area & Grasp ART-XC ART-XC Effective area [cm2] Grasp [cm2 deg2] Grasp of 7 eROSITA telescopes is 3-4 x higher than 3 XMM-Newton telescopes in the energy range 0.3-2 keV! At energies 5-15 keV, ART-XC is taking over significantly. Towards A CTA FP7 Design Study

  21. Mission Concept • Three surveys are planned in the eROSITA mission: • All-Sky Survey:42000 deg2 in 1 year • Extragalactic Survey: 20000 deg2 in 2.5 years • Deep Survey: 200 deg2 in 1/2 year • Pointed Observations Towards A CTA FP7 Design Study

  22. 0.5-2 keV 2-10 keV Expect [450,120, 36, 10] AGN@z >[ 6, 7, 8, 9] • a factor of 30 deeper than ROSAT (0.5-2 keV) • a factor of 100 deeper than HEAO-1 (2-10 keV) • expect ~ 100,000 clusters, • 3.4 Mio AGN (0.5-2 keV) • 250,000 AGN (2-10 keV) • and > 100,000 stars The eRosita survey Towards A CTA FP7 Design Study

  23. ART-XC: an X-ray Concentrator • Concentrator Kumakhov optics, polycapillary glass, diameter of capillaries ~1 m, capillaries ~2·1010 • Energy range 5-80 keV, • FOV 465 keV- 2.880 keV • Effective area of optics ~1150 cm2 30 keV • Energy resolution 1 keV 60 keV , • Grasp 150 deg2*cm2 10 keV Faint spectroscopy at Hard X-rays Obscured sources (AGN and more) Cosmic Hard X-ray Background Ti-44 line in SNR Hard spectra of Binaries Towards A CTA FP7 Design Study

  24. Lobster: all the sky, all the time Monitor Sun sensor Optic Module Star Tracker Front Back • Wide field X-ray monitor, 6 modules (60 MCP), FOV 22.5162 • 0.1 - 4.0 keV (TBD) • Angular resolution 4 (FWHM) • Energy resolution E/E 20% • a grasp 104 cm2 deg2 at 1 keV • 0.15 mCrab for day 4.000 Transients at 10-10 erg cm-2 s-1 36.000 at 10-11 erg cm-2 s-1 Daily Monitoring 400 AGN, typical timescales Catalogue: 250.000 sources • Consortium: UK (hardware) LU and MSSL, (science) Southampton. Finland U of Helsinki, Switzerland ISDC, Netherland SRON, Italy (GRBM), Spain? Towards A CTA FP7 Design Study

  25. Simbol-X a focusing telescope for hard X–ray astrophysics 0.5 – 80 keV formation flight Courtesy of Philippe Ferrando CEA/SAp & APC laboratory Towards A CTA FP7 Design Study

  26. Participating laboratories Short history F : CEA/Saclay, CESR/Toulouse, APC/Paris, LAOG/Grenoble, Obs.Paris/Meudon It : (INAF :) O.A.Brera, Roma, Palermo, IASF Milano, Bologna D : MPE Garching, I.A.A.Tübingen, Obs. Bamberg of Erlangen-Nuremberg Uni • End ‘01 : First ideas & discussions CEA/Saclay & O.A.Brera • End ‘03 : CNES call for scientific ideas using formation flight • Mid ‘04 : Selection of 4 missions for assesment phase (phase 0) • End ‘05 : Simbol-X recommended for phase A (alone) End ’06: Completion of Phase A Towards A CTA FP7 Design Study

  27. Eventually focusing at Hard X-ray! 30 arcmin XMM, Focusing Optics A pointed telescope with the XMM angular resolution and sensitivity in the INTEGRAL/ISGRI energy range 30 degrees INTEGRAL, Coded Masks Towards A CTA FP7 Design Study

  28. Major science goals Particle acceleration Mechanisms ? Maximum energy ? Accreting Black Holes Physics in single objects Census in Universe Towards A CTA FP7 Design Study

  29. Census of Super Massive Black Holes: where are the Obscured AGN ? ~50 % resolved in sources in the 7–10 keV band But less than a few % resolved beyond 10 keV CXRB models : major contribution from obscured AGNs, but parametres are not constrained (evolution, energy cut-off, absorption)  we need to resolve some of the 50% of the sources above 10 keV… Towards A CTA FP7 Design Study

  30. Accretion physics in Super Massive B.H. X-ray source « Secondary » components SIMBOL-X Black Hole Accretion disc access to quiescence state, and follow and characterize the change of state (« ADAF » vs jets ? Difference between neutron stars and black holes ?) V404 Cyg - Simbol–X 100 ks G.R. effects Towards A CTA FP7 Design Study

  31. With Simbol-X : • mapping of the synchrotron emission, • determination of spectral shape (and break) with X-ray alone • correlation with GeV and TeV emissions SX SX Towards A CTA FP7 Design Study

  32. Acceleration: electrons in SNRs shocks Simbol-X : E > 10 keV 100 ks / 10x15 arcmin2 SN1006 XMM 2-4.5 keV Spatially Resolved spectroscopy Towards A CTA FP7 Design Study

  33. other astrophysics topics… Explosive nucleosynthesis yield Cyclotron lines Young Stellar Objects Gamma-ray bursts follow up Non thermal cluster emission A2256/Beppo-SAX (Fusco-Femiano et al. 2000) Towards A CTA FP7 Design Study

  34. Simbol-X scientific requirements Continuum sensitivity [1 Ms, 3 ] : 10-14 erg/cm2/s [20-40 keV] (1μCrab) Line sensitivity : 10-7 ph/cm2/s @ 68 keV  Large effective area, excellent angular resolution, very low background Towards A CTA FP7 Design Study

  35. The only way to go : focusing With very long focal length possible thanks to formation flight Emax 1/θ Focal Length 20 to 30 m Low energy detector (450 mm Silicon) High energy detector (2 mm Cd(Zn)Te) Active anticoincidence shield Towards A CTA FP7 Design Study

  36. Hard X-ray Imaging(2 sets) EOB 9m F. L. (SXT) 12m F. L. (HXT) Hard X-ray Telescopes (2 sets) Soft X-ray Imaging(1 set) High Resolution Spectrometer (He dewar) Soft γ-ray detector SXS Soft X-ray Telescopes (2 sets) SXI HXI SGD NeXT mission (2012~) Hard X-ray Imaging + High resolution spectroscopy Energy 0.3keV 3keV 30keV 300keV Towards A CTA FP7 Design Study Slide from T. Takahashi, 2006

  37. 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 IMDC design Dec. 2004 e.g., EXIST measures Cen-A every orbit: characteristic time variability (QPOs) constrain BH mass http://EXIST.gsfc.nasa.gov • 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) Slides from J. Grindlay Towards A CTA FP7 Design Study

  38. MIRAX a Brazilian satellite SXI HXI(2) APS star camera Towards A CTA FP7 Design Study

  39. MIRAX SCIENCE Continuous broadband imaging spectroscopy of a large source sample (~9 months/yr) • Complete history of transient sources • X-ray bursts – superburst recurrence times and emergence of normal bursts after superbursts • Spectral state transitions and evolution on accreting compact objects • Accretion torques on neutron stars  accreting pulsars, pulsed period evolution, ms-pulsar recurrent outbursts • Relativistic jets on microquasars and other systems  X-ray light curves during radio ejections • Flaring X-ray sources and fast transients (many INTEGRAL sources) • Gamma-ray bursts (~1/month), especially XRFs  simultaneous X-ray AGs • AGN variability (obscured AGNs) Towards A CTA FP7 Design Study

  40. HXMT China's First X-ray Astronomy Satellite: Hard X-ray Modulation Telescope Mission Towards A CTA FP7 Design Study

  41. Integral HXMT Swift Before 2010, there is no other space astronomy mission approved internationally to have the capabilities of HXMT Angular Resolution 15’ < 5’ 14’ Source Location 2’ < 1’ 3’ Sensitivity (10^-7 / cm^2 s keV) 10 3 30 Observation Mode All sky survey no yes yes Selected sky deep survey yes yes no Narrow field pointing observation no yes no Towards A CTA FP7 Design Study

  42. Conclusions • The next decade will possibly be again a golden age in X-ray astronomy with many observatories in orbit • The main goals appears to be • A very deep survey of the soft-medium X-ray Universe for cosmology and astrophysics (eRosita) • A survey of the Hard sky (HXMT, EXIST) • The imaging of the Hard X-ray sky with soft-like sensitivity (Simbol X, NEXT) • Broad Band spectra / Timing studies (Spectrum X-Gamma, Simbol X, NEXT, MIRAX) • A deep “all sky all time” monitoring in the soft (Lobster, MAXI), medium-hard (Exist) , time variability of Binaries, AGN • Deep Study (Simbol X) and continous monitoring (MIRAX) of our Galaxy Towards A CTA FP7 Design Study

  43. Conclusions • These observatories will provide a perfect complement at soft-medium-hard X-ray to TeV Observations • Constraining SED in the broad X-ray band (… and therefore models!) • Providing detailed morphology in the broad X-ray band • Providing spatially resolved spectroscopy in the broad X-ray band • Allowing a continuous time monitoring of e.g. Blazars • To seek the collaborative support of the High Energy Astrophysics community at large for CTA is mandatory • As it is mandatory to shape CTA as an observatory, which is always the best way to maximize any scientific output… Towards A CTA FP7 Design Study

  44. Simbol X the Movie Towards A CTA FP7 Design Study

  45. Mission parameters for the newest configuration Towards A CTA FP7 Design Study

  46. X-ray Clusters for Precision Cosmology: six good reasons • Cluster mass function mainly depends on the matter density Wm and the amplitude of the primordial power spectrum s8 • Evolution of mass function N(z) gives sensitive constraints on DM and DE • Cluster Power Spectrum amplitude and shape depend on DM and DE • Baryonic Wiggles due to acoustic oscillations at recombination give tight constraints on space curvature • Cluster baryon fraction as a function of redshift provides constraints on DM and DE • Clusters provide direct distance measurements due to combined X-ray and SZ-measurements Courtesy of G. Hasinger (2006) Towards A CTA FP7 Design Study

  47. The new Spectrum-X-Gamma Mission • Launch in the 2010-2011 timeframe by Soyuz-2 • Two launch options, 600 km circular orbit: • Baikonur – inclination  30 as baseline • Kourou – inclination 5 as option • Medium size spacecraft: • Navigator (Lavochkin, under development, baseline) • Yamal (Energia, several similar S/C in operation) • Payload: • eROSITA(Germany), X-ray mirror telescopes • Lobster(UK), wide field X-ray monitor • ART(IKI, Russia), X-ray concentrator based on Kumakhov optics • GRB (IKI, Russia), gamma ray burst detector Towards A CTA FP7 Design Study

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