Early results of the Hitomi satellite

Hiro Matsumoto Ux group & KMI Nagoya Univ.1 Outline •Hitomi instruments •Early scientific results –DM in Perseus –Turbulence in Perseus

–others 2 Japanese history of X-ray satellites

Launch, Feb. 17, 2016 Weight Suzaku

Ginga ASCA Hitomi Tenma

Hakucho

Rocket

3 International collaboration More than 160 scientists from Japan/USA/Europe

4 Attitude anomaly  Loss of communication (Mar. 26, 2016)

spinning

Gave up recovery (Apr. 28, 2016)5 Hitomi Obs. List

Target Date Perseus Cluster of galaxies Feb. 25—27, 2016 Mar. 4—8, 2016 N132D Supernova remnants Mar. 8—11, 2016 IGR J16318-4848 Pulsar wind nebula Mar. 11—15, 2016 RXJ 1856-3754 Neutron star Mar. 17—19, 2016 Mar. 23—25, 2016 G21.5-0.9 Pulsar wind nebula Mar. 19—23, 2016 Crab Pulsar wind nebula Mar. 25, 2016

6 Scienfitic Instruments

7 4 systems Name X-Ray Telescope SXS Soft Micro-calorimeter (E<10keV) SXI Soft CCD (E<10keV) HXI Hard Si/CdTe (E<80keV) SGD --- Si/CdTe

(Compton) 8 Wide energy range (0.3—600keV) HXT 1keV∼ 107K SXT SGD SXI HXI SXS

9 SXT + SXS (0.3—12keV) Soft X-ray Telescope Soft X-ray Spectrometer (X-ray micro-calorimeter)

f=5.6m

10 Soft X-ray Spectrometer (SXS)

FOV: 3′ × 3′

Δ푇 ∝ ℎ휈 6 × 6 pix 11 Energy Resolution

Hitomi SXS Suzaku CCD

Δ퐸 = 5 푒푉@ 6푘푒푉 (cf. CCD Δ퐸 = 130 푒푉)12 Before Hitomi: gratings

Point source Extended

Not good for extended objects 13 X-ray microcalorimeter

Extended

Non-dispersive type. Spatial extension doesn’t matter. 14 X-Ray Telescope (SXT, HXT) Wolter-I optics

focus X-ray source

“Annual ring” of foils 15 Soft X-ray Telescope (SXT) 450mm

101.6mm

SXT-1 FM Au-coated Al foils 203 nested shells Total reflection

Angular resolution∼ 1.3′ 16 SXT + SXI (0.3—12keV) Soft X-ray Telescope Soft X-ray Imager (X-ray CCD)

f=5.6m

17 Soft X-ray Imager (SXI) Pch X-ray CCD

SXI

Thick depletion layer XMM ~200 um Moderate Δ퐸 Largest FOV (∼150eV@6keV) 38′ × 38′ 18 HXT + HXI (5—80keV) Hard X-ray Telescope Hard X-ray Imager (Si DSD + CdTe DSD)

f=12m

19 Hard X-ray Telescope (HXT) Made in Nagoya U.

HXT1 Wolter-I

62 kg 50cm

45 cm HXT2

1278 reflectors

20 HXT mirror Pt & C multilayer

21 Hard X-ray Imager (HXI) E<20 keV: Double-sided Si Strip Detector E>20keV: Double-sided CdTe Strip Detector

FOV: 9′ × 9′22 SGD (10—600keV)

Soft Gamma-ray Detector (Si+CdTe)

23 Soft Gamma-ray Detector (SGD)

• Si/CdTe Compton Camera • Active shield of BGO

24 Scienfitic Results

25 X-ray vs Visible Perseus cluster of galaxies

X-ray Optical

20M lyr Fabian et al. 2011, MNRAS, 418, 215426 Filled with Hot Gas

푘푇 ∼ 5푘푒푉 27 Main Component: Hot Gas

푀𝑔푎푠 > 푀𝑔푎푙 28 Trapped in DM potential

29 Perseus with XMM-Newton Bulbul et al. 2014

30 unID line at 3.5 keV

Not an atomic X-ray line

DM 푚퐷푀 ∼ 7푘푒푉 decay? Bulbul et al. 201431 Hitomi Calorimeter Hitomi collaboration, arXiv:1607.07420

32 No detection Hitomi collaboration arXiv:1607.07420

33 Why still hot?

2 × 105 퐿푦푟

Gas should cool within 2 × 109 yrs

34 Active Galaxy NGC1275 35 Active Galactic Nucleus Super-massive BH

36 Jet BH

Accretion Disk

Very hotX-ray 37 BH puts energy into gas?

38 Distrubed?

http://kakaku.com/article/pr/14/02_sharp_es-tx930/39 Perseus with Hitomi

Hitomi collaboration Nature 2016, 535, 117

40 Iron line: Outer region Broadened due to Doppler v = 164 ± 10 푘푚 푠−1

41 Turbulent velocity Outer reg. 164 ± 10 푘푚/푠 Center reg. 187 ± 13 푘푚/푠

푃푡푢푟푏 ∼ 0.04 × 푃푡ℎ푒푟푚푎푙

42 푷풕풖풓풃 ∼ ퟒ% 풐풇 푷풕풉풆풓풎풂풍

Very quiet 43 hydrostatic equilibrium of gas

Hot gas distribution  Gravitational potential  DM distribution 44 Can BH heat gas? 2 × 105 퐿푦푟

Cool within 2 × 109 yrs

45 Can BH heat gas? Central region cools within 2 × 109 yrs 2 × 105 퐿푦푟

How much turbulence should be input?

푃푡푢푟푏 ∼ 4% 표푓 푃푡ℎ푒푟푚푎푙 46 Same Problem

200L 8L How fast does Out of the bath he put water? in 3 minutes. Ans: 3 min×4% = 7.2 sec 47 Can BH heat gas? Central region cools within 2 × 109 yrs 2 × 105 퐿푦푟

2 × 109 푦푟푠 × 4% = 8 × 107 푦푟푠 BH should put energy every 8 × 107 푦푟푠. 48 Can BH heat gas? Central region cools within 2 × 109 yrs 2 × 105 퐿푦푟

Energy has to go 2 × 105 퐿푦푟 within 8 × 107 푦푟푠.  푣 ∼ 700 km s−1 49 Can BH heat gas? Central region cools within 2 × 109 yrs What happens?2 × 105 퐿푦푟 New problem.

−1 −1 푣 ∼ 700 km s ≫ v푡푢푟푏 ∼ 160 푘푚 푠 Energy cannot spread! 50 퐹푒25+ 퐹푒24+ lines suppressed? 퐾훼 Why?

퐹푒24+ 24+ 퐾훼 퐹푒 퐾훽

51 Effect of optical depth?

퐹푒25+ 퐾훼

퐹푒24+ 퐾훼, 퐾훽 Possibility to measure the size of the cluster along the line of sight. 52 06 July 2016, Nature53 Another topic: Crab Optical X-ray

Supernova in 1054 54 supernova remnant Cassiopeia A SN1006

(movie)55 퐴푟16+ 퐹푒24+ 푆𝑖12+ 푀푔10+ 푆𝑖13+ 14+ 퐶푎18+ 푀푔11+ 푆 푆15+

Highly ionized ionshot gas 56 Crab spectrum Tavani+2011 No atomic line from radio to gamma Synchrotron emission

57 Crab spectrum Tavani+2011

Where is hot gas?

58 Crab with Hitomi

Emission/absoption lineCalorimeter search. spectrum

2 3 5 10 12 Energy (keV) 59 About HXT: Success!

Pulsar wind nebula G21.5-0.9 5-80keV 5-10keV 10-20keV

20-30keV 30-50keV 50-80keV

60 G21.5-0.9: Pulsar Wind Nebula

Chandra X-ray image@CXC

Pulsar J833-1034

P=61.86ms

B=3.6e12 G arcmin

6.3 6.3 PWN Accelerates electrons

Interstellar matter 61 What energy can electrons be accelerated to?

HXI G21.5

BGD

Any break in the spectrum? ©H. Murakami (U. of Tokyo)

62 Planned talks

Time Speaker Topics KMI2017 15:30, Jan. 6, 2017 T. Ohashi Perseus (Tokyo Metro. U.) and others 9:00, Jan. 7., 2017 T. Kitayama DM search (Toho U.) Seminar 16:00, Feb. 20, 2017 H. Yamaguchi Supernova Physics (NASA/GSFC)

63 Summary • Hitomi observed several objects. –Perseus, Crab, and others • Many scientific topics are under discussion.

Stay Tune! 64