Hitomi, the Perseus Cluster and AGN Feedback

Andy Fabian IoA Cambridge UKand the HITOMI COLLABORATION

a

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X-ray Calorimeter

Hitomi Soft X-Ray Telescope

Richard Kelley, Astro-H Summer School No. 6, Nara, August 2015 7

1624 reflectors 45 cm diam.43 kg

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 SpectrometerNovember 2015, Tsukuba Space Center, Japan(photos courtesy of JAXA)

Richard Kelley, Astro-H Summer School No. 6, Nara, August 2015 12

Energy Scale

5000

4000

3000

2000

1000

0

Count

s/0.5

eV bi

n

2800026000240002200020000180001600014000120001000080006000400020000Energy (eV)

Targets: Mn Fe KBr Cu GaAs Co Cr Ti Ag Mo ZnSe KCl Teflon (C,F) NaF MgF Si C,O Nb Sn

Ag K !

1

Ag K !

2 Ag K "

1,3

Ag K "

2

Mo K !

1

Mo K !

2

Mo K "

1,3

Zn K !

1

Zn K !

2

Zn K "

1 Se K !

1

Se K !

2

Se K "

1,3

Ti K !

1,2

Ti K "

1,3

Cr K !

1,2

Cr K "

1,3

Co K !

1,2

Co K "

1

Ga K !

1

Ga K !

2

Ga K "

1

As K !

1

As K !

2

As K "

1

Cu K !

1

Cu K !

2

Cu K "

1,3

Br K !

1

Br K !

2

Br K "

1,3 Fe K

!1,2

Fe K "

1,3

Mn K !

1,2

Mn K "

1,3

Sn K !

1

Sn K !

2

Sn K "

3

Sn K "

1

Sn K "

2

Nb K !

1

Nb K !

2

Nb K "

1,3

Mo K "

2

Nb K "

2

Br K "

2

Se K "

2 W L !

1

W L "

1 W

L "2 W L #

1

K K !1

K K " 1

Cl K !

1

Cl K "

1

Si K !

Si K "

Al K !

12

Al K "

Mg K !

Na K !

F K !

O K !

C K !

2500

2000

1500

1000

500

0

Count

s/0.5 e

V bin

592059105900589058805870Energy [eV]

Data Fit to LSF Natural line shape

LSF = 4.37 eV FWHM

Mn K !

1

Mn K !

2

4000

3000

2000

1000

0

Count

s/1 eV

bin

254002530025200251002500024900Energy (eV)

Data Fit to LSF Natural line shape

LSF = 14.5 eV FWHM

Sn K !

1

Sn K !

2

1600

1400

1200

1000

800

600

400

200

0

Count

s/0.5 e

V bin

11960119401192011900118801186011840Energy (eV)

Data Fit to LSF Natural line shape

LSF = 5.99 eV FWHM

Br K !

1

Br K !

2

FM Astro-H/SXS Detetor System

Performance of the flight model Astro-H Soft X-ray SpectrometerMeasured calibration data

Lots of spectral dynamic range!

Energy (keV)

H Moseley

Feb 17 2016JAXA HII-A

First de-mag to 50 mK on Day 5

Initial Operations

Shirron+2016… 9905-100 SPIESneiderman+2016… 9905-99 SPIE

Initial projected helium lifetime > 4 years

Also demonstrated cryogen-free mode during ground testing

Dete

ctor

Tem

pera

ture

(K)

50 mK

15

Mission lost due to operations mishap after 38 days!

!!!!!A#tude!Anomaly!!!!!!!1.!No!Sun!presence!!!!!!2.!Low!power!!!!!!3.!Temp!distribu=on!!!!!!!!!!!anomaly!

Good!Health!

Sequence!of!Event

MSP

MSP

MGN

MGN

3/26!!0313JST!

05:49JST! 07:31JST! 09:52JST! 16:40JST!

USC

USC

USC

USC

USC

No!radio!signal

3/25!2014JST !

JSPOC!Info

10:42JST±11M!

Breakup(es=mated)

HITOMI!status!

About!04:10JST

Presumed!=ne!when!the!a#tude!anomaly!occurred!(es=mated!!from!MSP!telemetry)

No!data!

Observa=on!Plan

RXJ\1856.5\3754

Crab!nebula Markarian205

A#tude!Maneuver!20:28\21:16!JST

A#tude!Maneuver!03:01\03:22!JST

Tracking!

2016.4.1

USCKTU!

Radio!signal!received

3/26!23:39JST

SNT

3/26!01:21JST

USC

3/29!0:33JST

3/28!21:58JST

USCKTU!

2 3 5 8

110

norm

aliz

ed c

ounts

s−

1 k

eV

−1

Energy (keV)

APEC model spectrum, T=5 keV

GV closed

GV open

Spectrum from wholearray

Perseus: Fe XXV (He-like) complex

BLACK: Hitomi SXS dataPURPLE: Hitomi SXS line response functionBLUE: Best previous spectrum (Suzaku CCD)

σturb = 164 ± 12 km s-1

Measured on 10 kpc scale

Gaussian turbulence

Pturb < 0.04 x Pthermal

Energy (keV)

Hitomi Collaboration, Nature 2016

5 eV energy resolution achieved in orbit, full array

~ 21,000 counts16 due to residual background

HEAD High Energy Astrophysics in the 2020’s and Beyond 23

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 theenergy! 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 DataThe 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 microcalorimeterspectroscopy 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

Temperatures

Chandra F+06

07

Hitomi Collaboration, Nature 2017Strong evidence for 2 types of Type Ia to produce the elements 35

Nature Paper 2

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

3.2 3.3 3.4 keV

Charge Exchange?

Future is XRISM (launch 2022) then