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X-ray Astronomy with High Spectral Resolution: Astro-E2 / ISAS

X-ray Astronomy with High Spectral Resolution: Astro-E2 / ISAS. Y. Tanaka. Detectors on Astro-E2. High resolution spectrometer (XRS) Cryogenic quantum calorimeter ΔE = 6 eV (FWHM) @ 6 keV imaging 3 ’diameter circle in 3 1 pixels. High throughput XRT + CCD (4) (XIS)

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X-ray Astronomy with High Spectral Resolution: Astro-E2 / ISAS

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  1. X-ray Astronomy with High Spectral Resolution:Astro-E2 / ISAS Y. Tanaka

  2. Detectors on Astro-E2 High resolution spectrometer (XRS) Cryogenic quantum calorimeter ΔE = 6 eV (FWHM) @ 6 keV imaging 3’diametercirclein 31 pixels High throughput XRT + CCD (4) (XIS) 1300 cm2 @ 6 keV comparable to XXM-Newton EPIC/pn advantage ofmuchlower background in orbit Hard X-ray dtector (HXD) ~ 10 – several 100 keV 330 cm2 @ 100 keV, best S/N so far

  3. Astro-E2: wide-band coverage X-ray Telescope Non-imaging detector PN 1000 XIS(4CCD) MOS(x2) HXD (GSO) ACIS Effective Area (cm2) 100 XRS HXD (pin) 10 1 10 100 Energy (keV)

  4. Astro-E2 X-ray Imaging Spectrometer XIS Soft X-ray Telescopes XRT GSFC ISAS Nagoya et al. Osaka Kyoto ISAS et al. X-ray Spectrometer XRS GSFC ISAS et al. Hard X-ray Detector HXD Tokyo ISAS et al.

  5. X-ray Spectrometer: XRS Cryogenic quantum calorimeter…….operated @ 60 mK NASA GSFC, ISAS et al. Life time: 2.5yr + 0.5yrwith ……mechanical coolerHighest spectral resolution……@>3 keV with large area CCD XRS

  6. Resolving power Effective area XRS HETG LETG XRS XRS RGS RGS HETG XRS Characteristics • XRS: Astro-E2 • RGS: XMM-Newton • HETG/LETG: Chandra x 6 XRS field of view 2.9' Powerful for diffuse sources Δv～100 km/s with Fe-K line

  7. Spectroscopy with XRS • Plasma diagnostics (He-like Fe-K lines resolved) • Abundances, and distribution of elements • Velocity fields (shock, bulk motion, turbulence etc.) • Fluorescence, absorption lines, reflection, Compton shoulder etc. Centaurus cluster: 100ksec He-like Fe-K line

  8. Perseus cluster Centaurus cluster Imaging cluster center 3'=40kpc 3'=60kpc Sanders, Fabian 02 • Ripple feature …(sound wave?) • Buoyant bubbles • Turbulence Thermal Fe-K 3000-5000 photons w z j k y x modify line structure Fabian et al. 03

  9. Line structure due to turbulence Simulated XRS Fe line profile1700 photons Inogamov & Sunyaev 03 ⇔Perseus: 50 ksec Turbulence Turbulences=200km/s Thermal Thermals=100km/s APEC 3 keV (1700 photons)s = 100 km/s (2.3 eV)s = 200 km/s (4.5 eV) line width accuracy: ±0.3 eV

  10. A754 (z = 0.054) Govoni et al.2004 contour=radio F.O.V. 3' ~ 200 kpc Merging clusters A3667 (z = 0.055) 1000 km/s A2256 (z = 0.058) 1000 km/s Δｖ= 500 km/s

  11. Diffuse X-ray Emission along the Galactic Ridge ASCA GC region excl.Sgr A l = 10° l = 28° Valinia et al. 1998 All the same spectral shape!

  12. Origin of GRXE ? Thermal model Fe-K lines simulated XRS spectrum f i r Line width & f /i /r : *Hot plasma ? *Charge exchange of …slow-down CR ions? *In-situ acceleration ?

  13. Sgr B2: giant molecular cloud near G.C. Emitting strong Fe-K fluorescence (6.4 keV) line. Interpreted to trace a past X-ray activity of Sgr A*. “Compton shoulder” simulation Time sequence after a flash Koyama et al. each shifted x1/20 Sunyaev & Churazov 1998 Watanabe et al. 2003

  14. Broad Fe K-line of AGN Broad red wing of Fe-line seen from several Sy1 with ASCA MCG-6-30-15XMM Vaughan & Fabian 2004 IC 4329AChandra HETGMcKernan & Yaqoob

  15. Resolving UTA of Photoionized Absorber simulation Photoionized Plasmas in Sy2 simulation NGC 1068

  16. Current status of Astro-E2 Integration & tests (June-December, 2004) All tests have been completed successfully. SA is ready for launch by the end December 2004. Launch schedule Launch originally scheduled in Feb. 2005 is delayed because H-IIa launch is given priority. Earliest window will probably be in June 2005.

  17. Observing time allocation AO-1… J = 3.9 Msec, ESA = 0.7 Msec SWG: Science Working Group, GO: Guest observer

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