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

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

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

4. Astro-E2: wide-band coverage 110100 Energy (keV) Effective Area (cm 2 ) 10 100 1000 XRS XIS(4CCD) HXD (pin) HXD (GSO) ACIS MOS( x 2) PN X-ray TelescopeNon-imaging detector

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

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

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

8. 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. He-like Fe-K line Centaurus cluster: 100ksec

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

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

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

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

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

14. 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” Watanabe et al. 2003 Sunyaev & Churazov 1998 Koyama et al. simulation each shifted x 1 / 20 Time sequence after a flash

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

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

17. Iron K line feature from Sy II Class A NGC 4151(50ks) Sy 1.9 Absorption features Variable Broad + Narrow Fe-K lines Double Gaussian T. Yaqoob Separation of narrow lines

18. 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.

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