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Hitomi, the 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) Energy Scale

Performance of the fight model Astro-H Soft X-ray Spectrometer Lots of spectral dynamic range! Measured calibration data

12 1 LSF = 14.5 eV FWHM ! Data Data ! LSF = 4.37 eV FWHM Fit to LSF

1

Fit to LSF 4000 ! 2500 Natural line shape

Al K Al Natural line shape Mn K

Sn K

2 2

! ! 2000 3000

1

!

Sn K Mn K Targets:

1500 1

Zn K Zn

! 5000 1 Mn 1600 ! Data LSF = 5.99 eV FWHM 2000 Fe Fit to LSF

Counts/1 eV bin Counts/1 eV KBr

Br K Ga K 1400 Natural line shape

Counts/0.5 eV bin Counts/0.5 eV 1000 Cu GaAs 1200 1000 Co

2 500 ! Cr 1000 Ti

Br K Ag 0 Mo 0 800 24900 25000 25100 25200 25300 25400 ZnSe 4000 Energy (eV) 1 5870 5880 5890 5900 5910 5920 KCl

!

Counts/0.5 eV bin Counts/0.5 eV 600 Energy [eV] Teflon (C,F) ! NaF

Cl K Cl 2 400

! MgF

1,2

2

Mg K Mg

! Si ! 200 C,O Zn K Zn Nb

Mn K

! Ga K 0 Sn 11840 11860 11880 11900 11920 11940 11960 Energy (eV) FM Astro-H/SXS Detetor System 1

Na K 3000 !

1

!

1

Sn K

!

!

1

!

1,2

1

!

!

F K

Mo K

Cu K

!

K K

1,2

!

Co K

Br K

C K

1

!

Cr K

1

2

!

!

!

1,2

Nb K Nb

!

2

Counts/0.5 eV bin Counts/0.5

!

As K

Cu K

2

2

O K O

!

!

!

1,2

2000 ! K Fe

2

1

1,3

Br K

!

1

"

!

"

Si K

1

Sn K

2

Mo K

Ti K Ti

!

!

1

Br K

Nb K Nb

"

Se K

1

Ga K

1,3

"

"

1

"

2

1,3

Ag K Ag

Se K

!

"

1,3

Zn K Zn

"

1

1,3

Co K

"

Se K

"

2

Sn K

1,3

!

"

As K

Ag K Ag

1

2

1,3

Cu K

!

"

1

1,3

"

1

As K

3

"

"

Mn K

1,3

"

2

"

"

2

1

Ag K Ag

Cr K

"

2

"

"

1,3

"

"

W L W

2 1000 Sn K

K K

W L W

Ti K Ti

2

Nb K Nb

"

"

"

Sn K

Mo K

Cl K Cl

Br K

Ag K Ag

Nb K Nb

Fe K Fe

1

#

"

Si K

Mo K

Se K

2

"

W L W

Al K Al

W L W

0 0 2000 4000 6000 8000 10000 12000 14000 16000 18000 20000 22000 24000 26000 28000 Energy (eV) Richard Kelley, Astro-H Summer School No. 6, Nara, August 2015 Energy (keV) 12 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! 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)

APEC model spectrum, T=5 keV 1 − keV 1 − GV open 1 10

normalized counts s GV closed

23 5 8 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 in the core of the Perseus cluster (Hitomi Collab.)

Hitomi Constraints on the 3.5 keV Line in the Perseus 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 NGC 1275: The first X-ray microcalorimeter spectroscopy of Fe-Kα line emission from an

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