Japan-China X-ray Astronomical Workshop @ ISAS/JAXA, Japan 19-21 Nov 2018 Analyses school: Suzaku(朱雀)/Hitomi(瞳) satellites Yukikatsu Terada (寺田幸功) Saitama Univ., Japan Japan-China X-ray Astronomical Workshop @ ISAS/JAXA, Japan 19-21 Nov 2018 Lecture plan Part I. (Introduction) 1. Audience assumed 2. X-ray astrophysical detectors 3. Suzaku and Hitomi satellites and on bard instruments ß We skip details of spacecraft Part II. (Analyses) 1. Preparation of analyses 2. Analyes software/caldb structure of Suzaku/Hitomi/XRISM 3. Instration of FTOOLs/CALDB 4. Suzaku/XIS analyses walk through 5. Suzaku/HXD analyses walk through 6. Hitomi/HXI analyses walk through Japan-China X-ray Astronomical Workshop @ ISAS/JAXA, Japan 19-21 Nov 2018 Part I. Introduction Japan-China X-ray Astronomical Workshop @ ISAS/JAXA, Japan 19-21 Nov 2018 1. Audience assumed Audience assumed: Beginners of Suzaku / Hitomi analyses, X-ray astrophysics educated. Q1. Knowledge on X-ray astrophysics: under-graduated graduated Ph.D No paper 1-2 paper(s) >5 paper(s) Q2. Knowledge on X-ray detectors: nothing user developer Q3. Analyses skills nothing user developer Poster session Please learn more. My targets, enjoy the school ! Enjoy sightseeing, See you in banquet. Japan-China X-ray Astronomical Workshop @ ISAS/JAXA, Japan 19-21 Nov 2018 2. X-ray astrophysical detectors Q. What is detector? E (energy) Q (charge) = PH (pulse height) Detector q (direction) x (position) what we want to know A. converter ! what we can get Physics process in conversion from E to Q ü Photo absorption ü Compton scattering In Suzaku area, we mainly use the photo absorption process. ü e+ e- pair creation In Hitomi, the Compton scattering process is used in hard band Havier materials can detect X-rays in higher energy band Materials Gas (Xe,Ar,..) 14Si, 32Ge, 48Cd, 53I, 83Bi Energy band (keV) 0.1 10 100 500 Detectors PC GSPC Photo Diode Ge CdZTe Scintillators DSSD CdTe (NaI, CsI) (GSO, BGO) Si pixel CCD Suzaku XIS/Hitomi SXI Suzaku HXD Hitomi HXI/SGD Japan-China X-ray Astronomical Workshop @ ISAS/JAXA, Japan 19-21 Nov 2018 3. Suzaku and Hitomi satellites The 5th and 6th series of the Japanese X-ray satellite 30m 20m 10m 内之浦宇宙観測所内之浦宇宙観測所 Hakucho Tennma Ginga ASCA Suzaku Hitomi XARM Ohsumi はくちょう てんま ぎんが あすか すざく ひとみ 大隈 (1979-1985) (1987-1991) (1993-2001) (2005-) (2016) (2020s) (1970) (1983-1989) 白鳥 天馬 銀河 飛鳥 朱雀 瞳 Chandra/Newton Athena Ufuru Einstein ROSAT (1970-73) (1978-91) (1990-99) Japan-China X-ray Astronomical Workshop @ ISAS/JAXA, Japan 19-21 Nov 2018 Energy coverage 1 keV 10 keV 100 keV 1 MeV 10 MeV 100 MeV 0.1 Hakucho 100 0.1 Temma 60 1 Ginga 500 0.4 ASCA 10 30 CGRO 30GeV 0.1ROSAT 2.4 0.1 BeppoSAX 300 2 RXTE 500 0.1 Chandra 10 0.1 XMM-Newton 15 30 AGILE 3 INTEGRAL 10 50GeV 0.2 Suzaku 600 10 Fermi 0.2 Swift 150 100GeV 0.2 MAXI 30 3 NuSTAR 75 0.2 ASTROSAT 100 0.2 Hitomi 600 1 HXMT 250 eROSITA XARM missing in 2020s.. Athena Japan-China X-ray Astronomical Workshop @ ISAS/JAXA, Japan 19-21 Nov 2018 3.1Suzaku satellite SKIP: Covered by Ishida-san’s talk Mirror CCDs Scintillator Mitsuda et al. 2007 PASJ 59 S1 Japan-China X-ray Astronomical Workshop @ ISAS/JAXA, Japan 19-21 Nov 2018 Suzaku Payload XIS XRT (X-ray mirror) (X-ray CCD camera) XRS HXD (X-ray micro calorimeter) Suzaku Payload in ISAS/JAXA Japan-China X-ray Astronomical Workshop @ ISAS/JAXA, Japan 19-21 Nov 2018 Suzaku detector team XRT (X-ray mirror) XIS (X-ray CCD camera) XRS (X-ray micro calorimeter) HXD Suzaku Payload in ISAS/JAXA Japan-China X-ray Astronomical Workshop @ ISAS/JAXA, Japan 19-21 Nov 2018 3.2 Suzaku XIS: Mirror + X-ray CCD (SKIP: we may skip details) Suzaku XIS is one of typical optical systems with a mirror + CCDs ASCA Chandra XMM-Newton Suzaku XIS0, XIS1, XIS3: Front Illuminated (FI) CCD XIS2: Backside Illuminated (BI) CCD (better for lower energy band) Japan-China X-ray Astronomical Workshop @ ISAS/JAXA, Japan 19-21 Nov 2018 Suzaku X-ray telescope (XRT) (SKIP: we may skip details) X-ray Mirror Diameter 40cm Focal length 4.75m（XRT-I） 4.5m(XRT-S) FOV（FWHM） 17’@1.5keV 13’@8keV Plate scale 0.724 arcmin/mm Effective area 440cm^[email protected] 250cm^2@8keV Angular resolution 2’（HPD) Japan-China X-ray Astronomical Workshop @ ISAS/JAXA, Japan 19-21 Nov 2018 (ref) X-ray CCDs, general Charge Coupled Device (CCD) (SKIP: this is just an reference) photon (E) Charge cloud (Q) transfer clock Read out What is different from optical CCDs? CCD for optical observation 1 cloud = many optical photons (Q ∝ Flux) à Obtain Frame Image CCD for X-ray observation 1 cloud = 1 X-ray photon (Q ∝ Energy) à Event detection process on board. à Pick up events (3x3 or 5x5 pixels) Charge could be splited à Assign GRADE par each event We get (0) Time (1) center position and (2) PHs of neighbor & deposit pixels à RA,DEC à Energy Japan-China X-ray Astronomical Workshop @ ISAS/JAXA, Japan 19-21 Nov 2018 Clocking modes of Suzaku XIS(SKIP: we may skip details) photon (E) Charge cloud (Q) transfer clock Read out Currently, the Suzaku team does not operate P-sum Mode Full Window 1/4 Window option 1/8 Window option MCG6-30-15 Cen A 4U1626-67 Time resolution = 8 sec Time resolution = 2 sec Time resolution = 1 sec Japan-China X-ray Astronomical Workshop @ ISAS/JAXA, Japan 19-21 Nov 2018 Clocking mode and pile-up limit Pile Up (SKIP: we may skip details) photon1(E1) photon2(E2) Charge cloud (Q) Pile-up occurs when two photons comes transfer clock almost simultaneously. Q ∝ E1 + E2 Read out smaller pile-up effect ß quicker read out ß smaller imaging size or lower efficiency Japan-China X-ray Astronomical Workshop @ ISAS/JAXA, Japan 19-21 Nov 2018 Suzaku XIS: Charge injection technique (SKIP: we may skip details) Space Environment (Cosmic-ray irradiation) à degradation of CCD sensor Charge Transfer Inefficiency (CTI) Ozawa et al., 2009; Bautz et al., 2004; Uchiyama et al., 2009; Nakajima et al., 2008 Degradation of Charge transfer à lower PH & worse energy resolution Peak Width Spaced-row Charge Injection (SCI) From 2006 Idea) Degradation of charge transfer ß increase of charge trap ß Put artificial charge before transferring a signal charge! Before SCI After SCI XIS2 frame image FWHM On ground (Artificial lines are removed in the off-line analyses) Nakajima et al., 2008 The gain (energy scale) is well calibrated within 5 eV errors! Japan-China X-ray Astronomical Workshop @ ISAS/JAXA, Japan 19-21 Nov 2018 Suzaku XIS: contamination (SKIP: we may skip details) XIS sensor Out gas from onboard instruments (C, N, O, H) will contaminated on the XIS optical blocking filter (OBF). à Absorb X-rays ! à Quantum efficiency below 2 keV decreases. Koyama et al., 2007 ~20℃ OBF CCD -90 ℃ This effect should be taken into account in the analyses (Ishisaki et al. 2007). Japan-China X-ray Astronomical Workshop @ ISAS/JAXA, Japan 19-21 Nov 2018 Suzaku XIS Operation Japan-China X-ray Astronomical Workshop @ ISAS/JAXA, Japan 19-21 Nov 2018 3.3 Suzaku HXD: Design concept The HXD is a scintillation counter (SKIP: Covered by Fukazawa-san) E crystal PMT Q ∝ E PH ∝ E Scintillation light Non-Imaging Spectrometer High sensitive scintillator = Reduce Background Background in orbit Phosphor sandwich scintillator X-ray background Narrow field of view Cosmic-ray X-rays from other object (direct (Cosmic X-ray background activation) Galactic diffuse Reject X-ray bgd stray from other objects etc) signal signal scintillator scintillator scintillator scintillator Detectors response X-ray from the object, but escaped by Compton scintillator Particles scattering from the earth Anti coincidence detectors (Reject NXB, Non X-ray background(NXB) reject Comptonized events) Japan-China X-ray Astronomical Workshop @ ISAS/JAXA, Japan 19-21 Nov 2018 Suzaku HXD Sensor (SKIP: Covered by Fukazawa-san) Side view Optical axis Top view Photo absorber PIN diodes GSO crystal Passive Collimator Anti coincidence BGO crystals こここここここここここここ Takahashi et al PASJ 2007 Kokubun et al PASJ 2007 16+20 Units Japan-China X-ray Astronomical Workshop @ ISAS/JAXA, Japan 19-21 Nov 2018 Suzaku HXD Performance(SKIP: Covered by Fukazawa-san) Takahashi et al PASJ 2007 Kokubun et al PASJ 2007 Sensitivity at 10-6 level. Japan-China X-ray Astronomical Workshop @ ISAS/JAXA, Japan 19-21 Nov 2018 Suzaku HXD data (cleaned) What you get is the hard X-ray spectrum. ③ ② ① ①PHA to Energy (gain calibration, non-linearity correction) ②Effective area and efficiency Energy response ③Estimation of non X-ray background Japan-China X-ray Astronomical Workshop @ ISAS/JAXA, Japan 19-21 Nov 2018 (SKIP: we may skip details) ① Suzaku HXD: Energy scale calibrationp 1 signal annihilation 2 GSO 3 intrinsic p a activation 1 GSO of 153Gd GSO 2 Cross-calibration between PIN&GSO Cyclotron absorption feature activation p of 152Gd 1 PIN GSO GSO 2 60usec delayed event Japan-China X-ray Astronomical Workshop @ ISAS/JAXA, Japan 19-21 Nov 2018 Suzaku HXD: ③ Variable NXB (SKIP: covered by Fukazawa-san’s talk) Suzaku orbit: SAA passage Map of Suzaku HXD-PIN UD count rate target Suzaku Low COR 550km Japan Low COR SAA South Atlantic Anomaly One-day Light Curves of surrounding units Accumulation of activation BGD 1 day 1 orbit Kokubun et al PASJ 2007 Japan-China X-ray Astronomical Workshop @ ISAS/JAXA, Japan 19-21 Nov 2018 Suzaku HXD: NXB modeling (SKIP: Covered by Odaka-san’s talk/Fukazawa-san’s talk) Variable NXB à No rocking system (src ⇔ bgd) = No real time data à Estimation of NXB Two approaches in estimation of NXB 1.