The Suzaku mission Kazutaka Yamaoka Aoyama Gakuin University

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

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

Suzaku launch u u u Fifth Japanese-US X-ray satellite Launched by M-V rocket on July 10, 2005 Astro-E 2 Suzaku (朱雀) “red Chinese phoenix” u LEO 570 km, 31 deg.

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

Current Status of Suzaku 2005 July 10 th Launch of Astro-E 2 2005 Aug. 8 th XRS accident 7 e. V@6 ke. V at 60 m. K 2005 Aug. 12 th First light of XIS (E 0102 -72) 2005 Aug. 19 th First light of HXD (Cen A) 2005 Sep. 1 st Start of PV observations (SWG) ～ 70 sources 2006 Apr. 1 st Start of GO observations (AO 1) ～ 2007 Mar. AO 2 (the proposal due date will be Dec. 2006)

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

Hard X-ray Detector (HXD) Well-type GSO/BGO phoswich detectors + Si PIN diodes with 2 mm thickness u Narrow field of view 0. 5°× 0. 5°<100 ke. V u Thorough active shielding surrounded with BGO u First Japanese hard X-ray instrument u

HXD background rejection u Power of active shielding HXD-GSO

HXD background level u The lowest background is achieved. The sensitivity depends on modeling of the background. Current: 5% accuracy ～ 0. 5 m. Crab in 10 -40 ke. V u Crab RXTE Beppo-SAX/PDS Suzaku/HXD Background study is still in progress Our Goal: 1% ～ 0. 1 m. Crab level GSO PIN Energy (ke. V)

Key science of Suzaku u Wide-band spectroscopy 0. 2 -600 ke. V • Variable Galactic and extragalactic sources • Unidentified IGR sources and Ge. V/Te. V sources “provide exactly simultaneous data” u u 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

Suzaku performance (I) - X-ray response Iron-Kα S XV Kβ center Si XIV Kα Si XIII Kβ S XV Kα S XVI Kα Si XIII Kα u Galactic ASCA 320 ksec (Koyama et al. 1996) Iron-Kβ, 　 Ni-Kα Chandra 600 ksec (Muno et al. 2004) Suzaku 180 kec Preliminary! Koyama et al. XMM 50 ksec (Tanaka)

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

Cyclotron resonance features in the magnetized neutron stars u Her X-1 and transient pulsar A 0535+262 Preliminary! ～ 37 ke. V ～ 46 ke. V Terada, Mihara et al.

Galactic black hole binaries u u Low/hard state of Cyg. X-1 and GROJ 1655 -40 Study of corona, disk and reflected material Ratio to wabs 0. 5* PL(Γ=1. 6) Each 20 ksec soft excess narrow Fe (6. 4 ke. V) 0. 5— 350 ke. V Cutoff (Te=110 ke. V) Kubota, Takahashi et al. Preliminary!

Microquasar GRS 1915+105 (I) u Large multi-wavelength Campaign on Oct. 18 -19 INTEGRAL, Swift, RXTE Spitzer, ESO-NTT XIS (1 -12 ke. V) VLA, Ryle etc. . u Oscillation state PIN (10 -40 ke. V) Ueda et al.

Microquasar GRS 1915+105(II) u Study of hard X-ray behavior in the state variations Absorption-line changes with intensity variations. Oscillation High H-like iron-K Stable Oscillation Low Preliminary! Ueda et al.

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

Wide-band study of AGNs u Study of reflection and high energy cutoff in the AGNs CXB synthesis Preliminary! NGC 2110 Ecut>150 ke. V No reflection? Okajima et al. MCG 5 -23 -16 Reeves et al.

Radio galaxy 3 C 120 Suzaku compared to Beppo. SAX 1 10 Beppo SAX (160 ksec) Zdziarski & Grandi, 2001 100 Kataoka et al. Good S/N Preliminary! Suzaku (150 ksec)

Wide-band All-sky Monitor (WAM) u Second function of HXD lateral shield e. x. Beppo-SAX GRBM, INTEGRAL SPI-ACS n n Large effective area 400 cm 2 @1 Me. V Wide field of view Ideal GRB detectors !

GRB light curves u u 83 GRB candidates per 8 months WAM detection rate: ～ 120/year short/long bimodal distribution short Preliminary! long WAM 0. 2 s 30 s

WAM energy spectra Me. V emissions were detected from some GRBs ! Study of Me. V emission GRB 051008 GRB 060213 GRB 060317 Me. V emission !

WAM + Swift/BAT spectra u u Suzaku/WAM 50 -5000 ke. V Swift/BAT 15 -150 ke. V Broadband coverage 15 -5000 ke. V Suitable for study of prompt emissions GRB 051008 GRB 051111 GRB 050915 B

High red-shift GRB 050904 u u Most distant z=6. 29 T 90: 212 s WAM Ep=201 (-43, +84) ke. V Preliminary! WAM BAT

Short hard GRB 051221 A u u z = 0. 54 T 90: 0. 22 s Ep=378 (-120, +285) ke. V WAM BAT Preliminary!

Amati relation in the WAM-GRBs 7 GRBs z GRB 050904 6. 29 GRB 051109 A 2. 346 GRB 051111 1. 55 GRB 051221 0. 54 GRB 060210 3. 91 GRB 060223 A 4. 41 GRB 060502 A 1. 51 Preliminary!

IPN localizations WAM joined the 3 rd Interplanetary Network since Jan. 2006 u Localize the short/hard burst as fast as possible follow-up with Swift/XRT or optical telescopes Konus-WAM u GRB 060213 GRB 060303 GRB 060317 GRB 060425 GRB 060429 GRB 060522 GRB 060610 Konus-SPI-ACS Konus-MO GRB 060610

Summary u The X-ray satellite Suzaku is now operating well with two instruments (XIS and HXD) ★Power of “Suzaku” u u 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.

Suzaku conference u Kyoto, Japan u Dec. 4 -8, 2006

Te. V SNR RXJ 1713 -3946 HXD Narrow FOV First Detection up to 40 ke. V Preliminary! XIS 0 HXD-PIN XIS Takahashi, Tanaka et al. HXD　47. 8 ksec 40 ke. V

Compton thick AGNs u NGC 4945 Griffith, Isobe, Itoh et al.

Epeak Distributions Number of events -WAM results -normalized BATSE results Ep (log)

HXD Expected Sensitivity 3 x 10 -11 erg/s/cm 2 (10 -100 ke. V) 3 x 10 -12 Continuum Sensitivity 　d. E/E = 0. 5 　Exp. = 100 ks 　3 sigma stat. 1 and 3 % of BGD ・ 10 -30 ke. V, 3 sigma photon limit for 100 ks : 0. 1 m. Crab ・ 10 -30 ke. V, 　２% of BGD : 0. 1 m. Crab The better modeling of backgrond will allow fainter source, 0. 1— 0. 2 m. Crab at 10— 40 ke. V.