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The Suzaku mission

The Suzaku mission. Kazutaka Yamaoka Aoyama Gakuin University On behalf of the Suzaku team. Outline of my talk. Suzaku overview : instruments and current status Early results from PV phase Galactic X-ray binaries, AGNs, … Suzaku wide-band all-sky monitor (WAM) GRB prompt emissions.

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The Suzaku mission

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  1. The Suzaku mission Kazutaka Yamaoka Aoyama Gakuin University On behalf of the Suzaku team

  2. Outline of my talk • Suzaku overview : instruments and current status • Early results from PV phase • Galactic X-ray binaries, AGNs, … • Suzaku wide-band all-sky monitor (WAM) • GRB prompt emissions

  3. Suzaku launch • Fifth Japanese-US X-ray satellite • Launched by M-V rocket on July 10, 2005 • Astro-E2  Suzaku (朱雀) “red Chinese phoenix” • LEO 570km, 31 deg.

  4. X-ray Telescopes XRT GSFC ISAS Nagoya X-ray Calorimeter XRS GSFC ISAS TMU Hard X-ray Detector HXD Tokyo ISAS RIKEN Suzaku instruments X-ray CCD Camera XIS MIT Osaka Kyoto ISAS

  5. Current Status of Suzaku 2005 July 10th Launch of Astro-E2 2005 Aug. 8th XRS accident 2005 Aug. 12th First light of XIS (E0102-72) 2005 Aug. 19th First light of HXD (Cen A) 2005 Sep. 1st Start of PV observations (SWG) ～70sources 2006 Apr. 1st Start of GO observations (AO1) ～2007 Mar. 7eV@6keV at 60mK AO2 (the proposal due date will be Dec. 2006)

  6. XRT+X-ray CCD(XIS) XIS: 3 FI chips + 1 BI chip • Large effective area around the iron band • Good line-response in the soft X-rays • Low background XMM Suzaku Suzaku BI Suzaku FI Chandra

  7. Hard X-ray Detector (HXD) • Well-type GSO/BGO phoswich detectors + Si PIN diodes with 2mm thickness • Narrow field of view 0.5°×0.5°<100keV • Thorough active shielding surrounded with BGO • First Japanese hard X-ray instrument

  8. HXD background rejection • Power of active shielding HXD-GSO

  9. Crab RXTE Beppo-SAX/PDS Suzaku/HXD GSO PIN Energy (keV) HXD background level • The lowest background is achieved. • The sensitivity depends on modeling of the background.  Current: 5% accuracy ～0.5 mCrab in 10-40 keV Background study is still in progress Our Goal: 1% ～ 0.1 mCrab level

  10. Key science of Suzaku • Wide-band spectroscopy 0.2-600 keV • Variable Galactic and extragalactic sources • Unidentified IGR sources and GeV/TeV sources “provide exactly simultaneous data” • Study of x-ray emissions for diffuse sources • Plasma diagnostics with high energy resolution Search for the hard X-ray tail  Connections between thermal and non-thermal universe

  11. Suzaku performance (I)- X-ray response - Iron-Kα • Galactic center ASCA320 ksec (Koyama et al. 1996) Iron-Kβ, 　Ni-Kα S XV Kβ S XVI Kα S XV Kα Si XIII Kβ Si XIV Kα Si XIII Kα Chandra600ksec (Muno et al. 2004) Suzaku 180 kec Preliminary! Koyama et al. XMM 50 ksec (Tanaka)

  12. Suzaku performance - Wide-band spectroscopy - • Spectral study for weak sources (a few mCrab) Preliminary! Cen A “HXD first light !” Watanabe et al.

  13. Cyclotron resonance featuresin the magnetized neutron stars • Her X-1 and transient pulsar A0535+262 Preliminary! ～37 keV ～46 keV Terada, Mihara et al.

  14. Galactic black hole binaries • Low/hard state ofCygX-1 and GROJ1655-40 • Study of corona, disk and reflected material Ratio to wabs0.5* PL(Γ=1.6) Each 20 ksec soft excess narrow Fe (6.4keV) 0.5—350 keV Cutoff (Te=110keV) Preliminary! Kubota, Takahashi et al.

  15. Microquasar GRS1915+105 (I) • Large multi-wavelength Campaign on Oct. 18-19 INTEGRAL, Swift, RXTE Spitzer, ESO-NTT VLA, Ryle etc.. • Oscillation state XIS (1-12 keV) PIN (10-40 keV) Ueda et al.

  16. Microquasar GRS1915+105(II) Absorption-line changes with intensity variations. • Study of hard X-ray behavior in the state variations Oscillation High H-like iron-K Stable Oscillation Low Preliminary! Ueda et al.

  17. MCG 6-30-15 XIS • Broad-iron line associated with absorption lines confirmed • Less variable in hard X-rays Preliminary! Fabian et al.

  18. Wide-band study of AGNs • Study of reflection and high energy cutoff in the AGNs  CXB synthesis Preliminary! MCG5-23-16 NGC2110 Reeves et al. Ecut>150keV No reflection? Okajima et al.

  19. Radio galaxy 3C120 Kataoka et al. Suzaku compared to BeppoSAX Good S/N 100 1 10 Preliminary! Beppo SAX (160ksec) Suzaku (150ksec) Zdziarski & Grandi, 2001

  20. Wide-band All-sky Monitor (WAM) • Second function of HXD lateral shield e.x. Beppo-SAX GRBM, INTEGRAL SPI-ACS • Large effective area 400cm2 @1MeV • Wide field of view • Ideal GRB detectors !

  21. GRB light curves • 83 GRB candidates per 8 months  WAM detection rate: ～120/year • short/long  bimodal distribution Preliminary! short long WAM 0.2s 30s

  22. WAM energy spectra MeV emissions were detected from some GRBs !  Study of MeV emission GRB051008 GRB060213 GRB060317 MeV emission !

  23. WAM + Swift/BAT spectra • Suzaku/WAM 50-5000 keV • Swift/BAT 15-150 keV • Broadband coverage 15-5000 keV Suitable for study of prompt emissions GRB051008 GRB051111 GRB050915B

  24. High red-shift GRB 050904 • Most distant z=6.29 • T90: 212 s Ep=201 (-43, +84) keV Preliminary! WAM WAM BAT BAT

  25. Short hard GRB 051221A Ep=378 (-120, +285) keV • z = 0.54 • T90: 0.22 s WAM WAM BAT BAT Preliminary!

  26. Amati relation in the WAM-GRBs z GRB050904 6.29 GRB051109A 2.346 GRB051111 1.55 GRB051221 0.54 GRB060210 3.91 GRB060223A 4.41 GRB060502A 1.51 7GRBs Preliminary!

  27. IPN localizations • WAM joined the 3rd Interplanetary Network since Jan. 2006 • Localize the short/hard burst as fast as possible  follow-up with Swift/XRT or optical telescopes Konus-WAM Konus-SPI-ACS GRB060213GRB060303GRB060317GRB060425GRB060429GRB060522GRB060610 Konus-MO GRB060610

  28. Summary • The X-ray satellite Suzaku is now operating well with two instruments (XIS and HXD) ★Power of “Suzaku” • Wide-band coverage • Soft X-ray response and very low background • WAM as a monitor of GRB prompt emissions cf. Suzaku pointing  afterglow study • The exciting results will be presented at the Suzaku conference in Kyoto on Dec. 2006.

  29. Suzaku conference • Kyoto, Japan • Dec. 4-8, 2006

  30. XIS0 HXD-PIN 40 keV TeV SNR RXJ1713-3946 HXD Narrow FOV First Detection up to 40keV Preliminary! XIS HXD　47.8ksec Takahashi, Tanaka et al.

  31. Compton thick AGNs • NGC4945 Griffith, Isobe, Itoh et al.

  32. Epeak Distributions Number of events • WAM results • normalized • BATSE results Ep (log)

  33. HXD Expected Sensitivity 3x10-11 erg/s/cm2 (10-100 keV) Continuum Sensitivity dE/E = 0.5 　Exp. = 100 ks 　3 sigma stat. 1 and 3 % of BGD 3x10-12 ・10-30 keV, 3 sigma photon limit for 100 ks : 0.1 mCrab ・10-30 keV, 　２% of BGD : 0.1mCrab The better modeling of backgrond will allow fainter source, 0.1—0.2 mCrab at 10—40 keV.

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