High-resolution X-ray spectroscopy
with XARM
andfuture mission candidate FORCE for
hard X-ray/wide-band imaging spec.
Kazuhiro Nakazawa
on behalf of the XARM team and the FORCE WG

Vision for XARM and future hard X-ray
Hitomi SXS “Perseus spectra”

Hitomi HXI “Crab image”l Early recovery of high-resolution X-ray spectroscopy
Talk-1à the XARM missionl hard X-ray/soft gamma-ray road-map• HXI science only partly covered by NuSTARàcandidate “HXI recovery”: FORCE (late 2020 ‒ 2030).
Hard-band coverage in Athena/Lynx era Talk-2• SGD science uncovered à under consideration 	Talk-1: XARM
-the X-ray Astronomy
Recovery Mission-

Fe XXFe I

Mn XCr XXI

S (coun10.1

The Power of high-resolution
with	  2	  month	  X-ray spectroscopy
opera.on.	
0

5.5

6.0

6.5

7.0
E (observed) (keV)

7.5

8.0

8.5

7.5

8.0

8.5

1: The quiescentintracluster medium (Nature2016)
The tightest previous
all 1-arcmin-resolution bins have broadening of less than
km200s .
−1gas was from the XM
With just a single observation we cannot comment on how this result
giving11,12 an upper limit< 3 keV, wherek is Bolt
Perseus cluster oﬀ-center spectrakT
the distant luminous cla 2.0
for only a few peaked c
Fe XXV HeαInstrumental	
other bright clusters isz = 0.01756
from a slitless dispersi
1.5‒1v = 164 km s
spectrometer (the correHitomi SXS achieves mThermal (80 km/s)
to it being non-dispers
Thermal(80 km/s)
1.0
We measure a slightl
in the central regionFig.
(＋turbulenceThis region exhibits a s(164km/s)
0.5whichis several timeswith XMM-Newton, coChandra X-ray imagezyxw
other wavelengths. A
the spectrumFig.
( 1), wand Hitomi SXS FoV
06.50
6.55
6.60
cold gas present in theX線エネルギー(キロ電子ボルト)
slightly lower average t(4.1±0.1keV). By ﬁtting
bc
Heαr
0.3
Fe XXVI Lyα
Fe XXV Heβ
which is lower than thkT = 3.8keV, the currentof 2.8 and 2.9‒3.6) andS (counts s ‒1 keV ‒1)

Plasma subsonicmosiontranslateskinetic
to the wider clustercore.

• First clear determination of turbulence motion• low sub-sonic even in AGN-ICM interaction region

The Power of high-resolution
X-ray spectroscopy 2nd	  nature!!	
2: Solving the Ni over-abundance problem (Nature 2017)

Metal flourescence line diagnostics• First resolved the Fe-Kb and Ni-Ka emission• Cluster Fe-Ni abundance is consistent with Solarà Well-averaged metal abundance ratio?

XARM Science Objectives• structure formation of the Universe and evolution ofclusters of galaxies•

thermal, non-thermal and their dissipation mechanisms inclusters of galaxies à how clusters evolve?

• circulation history of baryonic matters in the Universe• trace baryon cycles and metak distribution history in theuniverse à how metals distributed?

• transport and circulation of energy in the Universe•

reveal matter and energy feedback by galaxies and activegalaxies à BH-Gal. co-evolution• new science with unprecedented high resolution X-rayspectroscopy•

pioneer new horizon of X-ray astrophysics with plasma
diagnostics, graviational-redshift measurement, etc…

XARM compared with Hitomi
Instrument

Hitomi XARMSoft X-raySpectrometer

SXS

X-ray microcalorimeter○○Soft X-ray Imager

SXI

X-ray CCD○○

Hard X-ray Imager

HXI

DSSiD /CdTeDSD○

Not
Onboard

Soft Gamma-rayDetector

SGD

Si/CdTe-pad
Comptoncamera○Not
Onboard7	

two XARM instruments
Instrument

FOV/pix

ΔE (FWHM @6 keV)

Resolve (XMA + X-ray
microcalorimeter)

2.9ʼ □ /6 x 6 pix

7 eV(goal 5 eV)

0.3 ‒ 12
keV

Xtend (XMA + X-rayCCD)

38ʼ □/
1280 x 1280 pix< 250 eV at EOL(< 200 eV at BOL)

0.4 ‒ 13keV

bandtwo other sub-teams	
Science Operations TeamScience Management Oﬃce

XARM Science Team andObservation program Concept• Science Team:• data-rights to all PV data
• scientists of the sub-teams + ~dozen “ParticipatingScientists” by JAXA,NASA,ESA.

• “PV phase collaborating scientists” : new!
• data-rights only to a speciﬁed PV targe• appointed ~1 year before the launch• Guest Observer Program:• After start-up & PV phase, Guest Observation
program starts	

XARM Time Frame
2000

2005

2010

2015

2020

2025

XMM-Newton (1999- )Athena(2028- )Chandra (1999- )Fermi (2008- )NuSTAR(2012- )Swift (2004- )US/Europe onlySuzaku
ASTRO-H/Hitomi

2030年

HXM (FORCE?)XARM(~FY2020)

US/Europe + Japan

Japan + international

ALMA (radio）
JWST (IR）CTA (TeV gamma-ray）
TMT (Opt/IR)
SPICA (IR)Status
The XARM team (now ~100 members from JP+US+ESA)
PM: H. Maejima, PE: K. Toda (JAXA), PI: M. Tashiro (Saitama U./JAXA),
NASA PM: L. Reichenthal, SE: J. Lobell, co-PI: R. Kelley (NASA)
Resolve (Calorimeter): R. Kelley (NASA) + Y. Ishisaki (TMU)
Xtend (CCD): K. Hayashida (Osaka)
Integrated team ofengineer
Science Operation Team: Y. Terada (Saitama)
sicentists
Science Team Lead: to be appointed soon

Key Mile stones / Scheduleü 2016/10
ü 2017/4
ü 2017/11
ü 2017/11
ü ~2018/4
ü ~FY2020

Preparation-team stand up
Mission Deﬁnition Review/System Requirement Review
Pre-Project start
Critical Design Review at NASA for Resolve(planned) Project start(planned) Launch

Project now actively ongoing to recoverhigh-resolution X-ray spectroscopy

Talk-2

the FORCE mission proposal- Focusing On Relativistic universe
and Cosmic Evolution -The power of Hitomi Hard X-ray Imager

10Hard X-ray
Telescope

Effective Area (cm 2 )100

HXI-1 total
NuSTAR FPMA
HXI-1 after layer selection

Area = largest ever

0.1

51020

Energydata(keV)

50

1000.01

HXI
10−3

Hard X-rayImager

normalized counts s−1 keV−1

NuSTAR

10−4

BGD = lowest everproperly worked in orbit
for 13 days

51020
Energy (keV)50x4-5 better sensitivitiy than
NuSTAR for extended sources

FORCE Conceptual Design• Focal length 10 m
• 3x super-mirror + imager pairs• ~2026 launch aim
Wideband Hybrid X-ray Imager (WHXI)ü new Si-det (SOI-CMOS) + CdTeü low BGD (e.g. Hitomi HXI)ü wide-band; 1-80 keV
ü > □7ʼ FoV

X-ray Super-mirrorü Si mirror @ NASAü super-mirror (US/Jp)ü Δθ <15” (c.f. NuSTAR is 60ʼʼ)ü Eﬀ. area 369 cm2 @30 keV

Satellite Systemü 1.2t-class14

Science-1
MissingObjective
BH survey
Main Science©	  ESO/M.	  Kornmesser	©	  NASA	©	  Ute	  Kraus	

Obsucured Super-Massive
BHs (>104 Mo）
Intermediate Mass
BH（102-4 Mo）

Isolated “unseen”
BHs（<102 Mo）

Resolving the number of “Missing BHs”,
to understand the cosmoligical evolution
history of stars, galaxies and clusters.

Importance of 1-80 keV band
• Hard X-rays see “true AGN Luminosity”, apart from SF• Complementary to IR + ALMA survey
Lile Wang @ Princeton

トーラス小ISAS/JAXA

トーラス大

bright in X-rays
1st Missing BH WS
but not in IR@ Kyoto
2017/11/6-7 N4945

Kawamuro, Ueda+16, Perez-Beaupuits+ 11, etc…

深く埋もれたAGNのスペクトル例

16

17

Ovservatory Science : e.g. Diﬀuse
The lowest BGD of Hitomo HXI can be “halved” @ 10 keVà FORCE cab be ideal for “extended hard X-ray source”
20.1

80 arcmin scaled background

1 mCrabと9ʼx9ʼのBGDの比較「すざく」より低い

0.01

1

NuSTAR FPM

ratio

SXI NXB+CXB

3倍
HXI NXB+CXB

0.1

10 3

normalized counts s 1 keV 1

NuSTARより低い

HXI-1 after layer selection

100

10 4

Nakazawa et al. 2016
5102050

Energy (keV)

ed over a radius of 4′ of the HXI1-S. That without layer selection
Also shown in black in comparison is that of the NuSTAR FPMA.
er the layer selection accumulated over 80 arcmin2 area (magenta).
STAR FPM, scaled from the NuSTAR proposal information.

ng the largest. Our preliminary results shows that the point

XIS NXB+CXB
2510Energy (keV)

20

18	

Ovservatory Science : e.g. Diﬀuse
The lowest BGD of Hitomo HXI can be “halved” @ 10 keVà FORCE cab be ideal for “extended hard X-ray source”
Particle Accelleration in SNR

内山+2007

1. Cutoﬀ of synchrotron emission
cooling? escaping? aging?
2. Local B ampliﬁcation, withgood resolution imaging
田中+2008 (すざく)2016/12/27	

New science ﬁeld, in collaboration
with radio, IR-optical, gamma,neutrino, and GW shall be persued.
内山+2007 Nature(Chandra)Improved performance of SOIPIXCMOS	  (low	  ρ	  Si)	  • Each pixel has its own trigger andanalogue readout.
• Time resolution ~1μsec andthrough-put >1kHz (e.g. anticoincidence for low BGD)
• BI with depletion >200μm

Insulator	  (SiO2)	  Sensor	  	  (high	  ρ	  Si)	  14mm	  Tsuru	  et	  al.	

2017	  Oct.	  
Co-­‐57	  XRPIX6E	  (PFZ)	  -­‐60℃	  VBB	  -­‐200V,	  VCo-­‐57	  bpw	  Fe-­‐Kα	  -­‐2.0V	  (6.4keV)	  Single	  Pix.	  Event	  8×8	  pix	  no	  gain	  corr.	  

Fe-­‐Kα	  (6.4keV)	  FWHM	  300eV	  Fe-­‐Kβ	  -­‐60℃	  (7.1	  keV)	  VBB	  200V,	  Vms	  -­‐1.0V	  Single	  Pix.	  Event	  8×8	  pix	  no	  gain	  corr.	  

ENC	  36e(rms)	  Fe-­‐Kβ	  14.4keV	  (7.1keV)	  Fe-­‐Kα,	  Kβ	  are	  resolved	  22mm	  Event-­‐Driven	  readout	  mode	  Cd-­‐109,	  Vbb=10V,	  	  Room	  Temp.	  
Event	  rate	  >	  500Hz	  is	  Conﬁrmed	  Initial results from Si-mirror (NASA)
Riveros et al. 2014,15,16,17

Key technology• Si optics (NASA/GSFC PI. W. Zhang)+ multi-layer (Jp/US)• Si optics 1-pair w/o multi-layer àΔθ = 3ʼʼ.4 HPD is demonstrated.
• Tests with multi-layer on-goingSummary• FORCE mission is a candidate hard X-ray/wide band
(1-80 keV) probe with 10”-15” mirror• Main goal is to count the numbers of “mission BHs”,
SMBH, IMBH, and isolated-Stellar Mass BH• Also with its very low BGD, a good hard X-ray (8-20AOPhase	keV) diﬀuse source observationA1can be done
2013.122014.3 preparation
2014.6
0.58 4 is 2019.3• Aiming at 2026
launch,actively on-going.
2015.122016.1

2016.314

2015.122016.1

2016.32.5

4.5 2023.3

2017.2
AO
2017.22017.52017.82017.52017.84.5 2023.3	
52025.3

2018.82013.122018.112014.3 2019.2
2014.6

1Phase
2.5
A1
10.58

2018.82015.122018.112016.1 2019.2
2016.32.5
15.5
2027.342021.3

2020.2
2015.122020.52016.12020.82016.31
2.5

5.5
4.5 2027.3
2023.32017.22017.52017.81

4.5 2023.3

542021.32025.32019.3