Hitomi, the Perseus Cluster and AGN Feedback Andy Fabian IoA Cambridge UK and the HITOMI COLLABORATION a b c X-ray Calorimeter Hitomi Soft X-Ray Telescope 1624 reflectors 45 cm diam. 43 kg Richard Kelley, Astro-H Summer School No. 6, Nara, August 2015 7 Detector Assembly (FM) Richard Kelley, Astro-H Summer School No. 6, Nara, August 2015 8 SXS Cryogenic System Richard Kelley, Astro-H Summer School No. 6, Nara, August 2015 9 Dewar Integration Richard Kelley, Astro-H Summer School No. 6, Nara, August 2015 10 Soft X-ray Spectrometer November 2015, Tsukuba Space Center, Japan (photos courtesy of JAXA) Richard Kelley, Kelley, Richard Counts/0.5 eV bin Lotsspectralof dynamic range! Astro 1000 2000 3000 4000 5000 - H Summer School No. 6, Nara, August 2015 School August No. Nara, 6, H Summer 0 0 C K! O K! F K! Na K! Mg K! 2000 Si K! Energy Scale Energy Al K" Si K" Al K Cl K!1 !12 Energy ( Energy Cl K"1 K K!1 4000 K K"1 Counts/0.5 eV bin 1000 1500 2000 2500 500 0 keV Ti K line shape Natural FittoLSF Data !1,2 5870 ) Ti K"1,3 5880 Cr K!1,2 6000 Energy [eV] Energy 5890 Mn K!2 Mn K!1,2 Cr K"1,3 5900 Fe K!1,2 Mn K"1,3 Mn K!1 LSF = 4.37 eVFWHM LSF = 4.37 Co K!1,2 5910 Fe K"1,3 8000 5920 Co K"1 Cu K!2 Cu K!1 Zn K!2 W L!1 Zn K!1 Cu K"1,3 Ga K!2 Ga K!1 10000 12 Zn K 1 " Performance ofthe Performance W L"1 Counts/0.5 eV bin W L "2 1000 1200 1400 1600 200 400 600 800 Ga K"1 0 As K!2 11840 As K!1 Natural line shape Natural line FittoLSF Data Se K 2 ! 11860 Se K!1 12000 11880 W L#1 Br K!2 Br K As K"1 !2 Energy (eV) Energy 11900 Br K!1 11920 Br K!1 Measured calibration data calibration Measured Se K"1,3 f Se K"2 Spectrometer Soft modelAstro-H ight X-ray 11940 LSF = 5.99 eVFWHM LSF = 5.99 Br K"1,3 11960 14000 Br K"2 Energy (eV) 16000 Nb K!2 Nb K!1 FM Astro-H/SXS Detetor System Detetor Astro-H/SXS FM Mo K!2 18000 Mo K!1 Nb K"1,3 Nb K"2 20000 Mo K"1,3 Mo K"2 22000 Ag K!2 Ag K!1 Counts/1 eV bin 1000 2000 3000 4000 24000 0 24900 Natural line shape line Natural FittoLSF Data 25000 Ag K"1,3 Sn K!2 25100 Sn K 2 ! (eV) Energy Sn K!1 26000 25200 Ag K"2 Sn K!1 25300 LSF = 14.5 eVFWHM 14.5 LSF = 25400 28000 Sn K"3 Targets: Sn K "1 Sn Nb C,O Si MgF NaF Teflon(C,F) KCl ZnSe Mo Ag Ti Cr Co GaAs Cu KBr Fe Mn Sn K"2 H Moseley Initial Operations First de-mag to 50 mK on Day 5 50 mK Detector Temperature (K) Temperature Detector Initial projected helium lifetime > 4 years Also demonstrated cryogen-free mode during ground testing Feb 17 2016 Shirron+2016… 9905-100 SPIE Sneiderman+2016… 9905-99 SPIE JAXA HII-A Mission lost due to operations mishap after 38 days! 15 Sequence!of!Event 2016.4.1 Observa=on!Plan Crab!nebula Markarian205 RXJ\1856.5\3754A#tude!Maneuver! A#tude!Maneuver! 20:28\21:16!JST 03:01\03:22!JST Tracking! 3/26!! 3/25!2014JST! 0313JST! 05:49JST! 07:31JST! 09:52JST! 3/26! 3/26! 3/28! 3/29! 16:40JST! 23:39JST01:21JST21:58JST0:33JST M U S U U U U U M M M USC USC S S S S S S S G G S N KTU! KTU! C C C C C P P N N C T No!radio!signal Radio!signal!received About! !!!!!A#tude!Anomaly!! 04:10JST HITOMI! !!!!!1.!No!Sun!presence! status! Good!Health! !!!!!2.!Low!power! No!data! !!!!!3.!Temp!distribu=on! Presumed!=ne! !!!!!!!!!!anomaly! when!the!a#tude! anomaly!occurred! (es=mated!!from! 10:42JST±11M! MSP!telemetry) JSPOC! Info Breakup(es=mated) normalized counts s−1 keV−1 1 10 23 5 8 GV open GV closed APEC modelspectrum,T=5keV Energy (keV) Spectrum from whole array Perseus: Fe XXV (He-like) complex 5 eV energy resolution achieved in orbit, full array ~ 21,000 counts σ = 164 ± 12 km s-1 turb 16 due to residual background Measured on 10 kpc scale Gaussian turbulence Pturb < 0.04 x Pthermal Energy (keV) BLACK: Hitomi SXS data Hitomi Collaboration, Nature 2016 PURPLE: Hitomi SXS line response function BLUE: Best previous spectrum HEAD(Suzaku High EnergyCCD) Astrophysics in the 23 2020’s and Beyond SXS 6x6 array = 3x3 arcmin ~60x60 kpc ~3.5PV measured in thick rims (Graham+08) M87 Centaurus General implications • Energy content due to small scale motions (turbulence) ~4% • Motions could be due to bubbles, sound waves, sloshing, cold front, turbulence. • Gas is relatively quiet for such an active region! • X-ray observations of clusters should be good as cosmological probes. Energy in "turbulence" is 4% thermal energy, Cooling time over region is 1-2 billion yr. Take 2 billion yr, then time to replenish energy is 8x107yr. Speed with which energy must flow to spread over whole region is 750 km/s. This is >>160 km/s and close to sound speed (~1000 km/s). Turbulence can’t propagate the energy! Therefore energy transported by sound waves? Consistent with data (F+17). See also talks by C Pinto and C Bambic… Top: simulated line profiles due to the effect of the displacement velocity of sound waves in the ICM of the Perseus cluster. A. C. Fabian et al. MNRAS 2017;464:L1-L5 © 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society Published Refereed Papers from the Hitomi Perseus Data The quiescent intracluster medium in the core of the Perseus cluster (Hitomi Collab.) Hitomi Constraints on the 3.5 keV Line in the Perseus Galaxy Cluster Solar abundance ratios of the iron-peak elements in the Perseus cluster Atmospheric gas dynamics in the Perseus cluster observed with Hitomi Measurements of resonant scattering in the Perseus Cluster core with Hitomi SXS Temperature structure in the Perseus cluster core observed with Hitomi Atomic data and spectral modeling constraints from high-resolution X-ray observations of the Perseus cluster with Hitomi Hitomi observation of radio galaxy NGC 1275: The first X-ray microcalorimeter spectroscopy of Fe-Kα line emission from an active galactic nucleus An X-ray spectroscopic search for dark matter and unidentified line signatures in the Perseus cluster with Hitomi (Tamura+) Resonance Scattering 07 Temperatures Chandra F+06 Nature Paper 2 Strong evidence for 2 types of Type Ia to produce the elements Hitomi Collaboration, Nature 2017 35 Most turbulence has velocity~100 km/s or less HST Fabian+08 Lim+12 Spectrum of these filaments is unlike anything in Galaxy, other than Crab and due to energetic particles (the hot gas?) Ferland+08/9 Charge Exchange? 3.2 3.3 3.4 keV Future is XRISM (launch 2022) then .