20200121_AGN Jet Workshop @Tohoku Univ.

Sub-arcsecond to m-arcsecond
Resolution X-ray Imaging of SMBH
with a novel method MIXIM
K. Hayashida (Osaka Univ./JAXA)+K. Asakura, T. Hanasaka, T. Kawabata, T. Yoneyama,
H. Noda, K. Okazaki, S. Sakuma, A. Ishikura, M. Hanaoka,
S. Ide, K. Hattori, H. Matsumoto, H. Tsunemi (Osaka Univ.),
H. Nakajima (Kanto-Gakuin Univ.), H. Awaki (Ehime Univ.),
J.S. Hiraga (Kwansei-Gakuin Univ.)1Angular Resolution is essential

4Log( Anglar Resolution[arcsec])

32
10

D=0.1mm

-1

D=1m

-2

D=10m
D=10km-3

D=10000km-4

Naked Eye-5

Galileo-6-12-10-8-6-4Log(Wavelength [m])

-202

4

Wide Wave Length Band is also essential

D=0.1mm
D=1m
D=10m
D=10km
D=10000km
Naked eye
Galileo
ALMA
GRAVITY
Herschel PACS
HST
HST
Spitzer
ChandraNuStarHitomiSGD
EHT
GALEX
XMM
SuzakuHitomi
EAVN

Log( Anglar Resolution[arcsec])

3
Suzaku2
1

Hitomi
NuStar
XMM

0Chandra-1

Spitzer
Herschel
ALMA
HST-2

VLT GRAVITY-3

EAVN-4EHT-5Angular Resolution is essential, again-6-12-10-8-6-4Log(Wavelength [m])-203
EHT collaboration

Grazing Incidence Mirror + X-ray CCD is the de facto
standard of X-ray Observatories since ASCA (1993)
Hitomi SXTPhoton Counting
Imaging Spectroscopy

Focal LengthChandra 1999-

XMM-Newton

1999-

Suzaku2005-2015

Hitomi SXIAthena 2032?12m

0.5’’ 7.5m
10m
15’’ ~5m
5’’2’• Angular resolution is exceptionally good for Chandra, 0.5’’.
• Better or similar resolution mirror is very difficult to make (cost etc).
• Satellites must be big when grazing incidence mirrors are employed.

Our challenge to this field consensus

MIXIM

4

Multi-Pinhole(Slit) Camera is the baseline•

http://blog.goo.ne.jp/hanahana
haru04/e/a8ef27218dee371313
6a89943109a431

STACK
these multiple
images in theanalysis

5Hayashida+2016

Multi Image X-ray Interferometer/Imager
Parallel Beam

X-ray Pixel Detector(CCD/CMOS）

Grating
Pitch

Image
WidthOpening
Fraction
DistanceStack• Only employ a Grating and an X-ray Pixel Detector• Image profile detected reflects the profile of the X-ray source.
• Stacking the image with a period of in the analysis, accurate
source profile is obtained.
• Image Width=/ = 0.4′′.

/Chandra Resolution with a 50cm size satellite ?

But, diffraction blurs the image significantly.

6But, but, Talbot Effect can be employed• Talbot Effect• Parallel Light through a grating makes Self Image of thegrating at periodic distances. (H.F.Talbot, 1836)• Explained with Diffraction and Interference (Rayleigh, 1881)• Hard X-ray Talbot Effect in experiment (P. Cloetens, 1997)• Talbot DistancePlainWave
Light

Talbot Carpet

Image fromWen et al. Advances inOptics and Photonics 5,
83–130 (2013)=1=2=3For l=0.1nm(12keV) X-rays and a =5mm pitch grating,
Talbot distance of =2 is 50cm

7

Multi Image X-ray Interferometer
Module (or Method,Mission) = MIXIM
Hayashida+ 2016,2018• X-ray Grating with >a few mm pitch and X-ray Imaging
Spectrometer• Select X-ray Events of which energy is within specific bandaround the Talbot condition .
• Band-pass of about 10% (for m=2; 20% for m=1) can be utilized.
Wider than Si-detector energy resolution of 2~3%. Good for Xray CCD and X-ray CMOS.

• Stacked Image tell us the X-ray source profilec.f. X-ray Talbot (-Lau) Interferometer Momose+(2003), Pfeiffer+(2006) for Phase
Contrast X-ray Imaging of Light Material

Figure from http://rsif.royalsocietypublishing.org/content/7/53/1665

Hoshino+ 2014 KONICA MINOLTA
8TECHNOLOGY REPORT Vol11• X-ray Gratings of a few mm pitch are fabricated and purchased.
• Pixel size of the detectors should be a few mm or smaller, while
X-ray CCDs pixel is 24mm or larger.
• Variety of CMOS pixel detectors designed for optical light.
• Some groups (Einstein Probe, FOXSI-3) succeeded in detecting
X-rays with optical CMOS with 11mm pixel.
• We employed GSENSE5130 4.25mm pixel in 2017 andGMAX0505 2.5mm pixel in 2018, both from Gpixel Co.
FWHM=170eV@5.9keV
at Room Temperature!!!
In Open Air
13mmDetection Layer ~ 5mm Thick

Small pixel size enables us to detect X-ray polarization
See Asakura+ 2019, JATIS, 5(3) and Poster #501

9Small Pixel→Photo-electron-Track→X-ray polarimetry
12.4keV24.8keV•24.8keV12.4keV

Asakura+2019
JATIS, 5(3)MF=7.63±0.07%@12.4keV
15.5±0.4%@24.8keV
10SPring-8
BL20B2 200m beam line
SPring-8 BL20B2花坂M論2017 Nov,Dec 2018 May, Jun (4.25mm) 2018 Oct,Dec (2.5mm)
Hayashida+2018 SPIE Proc.

d=9.6mm, f=0.2

d=4.8mm, f=0.2z

Monochromatic
Polarized

X-ray Beam

~ 200 mCMOS

Grating

Rotation
回折格子Stage

Optical Benchz

d=9.6mm,f=0.2,z=92cm Raw Frame Image 6s-exposure
Ex=12.4keV
Ex=10.0keV(m=1.0; meet Talbot condition)(m=1.24; NOT meet)

Following data were taken with exposure/frame of 0.1-1s with attenuator to prevent pileup

Event Extraction→Projection→Folding Ex=12.4keV
Folded Profile

Normalized Counts

Visibility=(MAX-MIN)/(MAX+MIN)
MAXWidth

d=4.8mm, z=46cm

Visib.=0.59(MAX+MIN)/2

θ=0.55’’MIN*) Two periods are plotted for display purpose

d=9.6mm, z=92cm
Visib.=0.88

θ=0.41’’d=9.6mm, z=184cm
Visib.=0.78

θ=0.26’’
13

Energy Dependence of Visibility

14

Energy Dependence of Visibility→Band Width
d=9.6mm,f=0.2, z=92cm
10%20%ｍ=2ｍ=115

SPring-8 BL20B2 2019 Jul
1. Test large z case to obtain smaller (better) Image width <0.1’’
2. First 2D imaging by stacking two 1D gratings diagonallyz=8.67m
CMOS 2.5mmpix

X-ray
BeamGrating
d=9.6mm, f=0.2

Vacuum Tube

Optical benchThis Image is flipped horizontally to explain the configuration

This Image is flipped horizontally to explain the configuration

16

Resolution <0.1’’ , best ever achieved with X-ray astronomical imagers
Grating
Synchrotron Souce d=9.6mm, f=0.2150um (0.15’’) elongation
along H-direction issuggested•200m
Ex=12.4keV

Visibility=0.91

Grating
d=9.6um, f=0.2

CMOS2.5mmpix

CMOS2.5mmpix

Projection

z=8.67m

Projection

200m

z=8.67m

Ex=12.4keV
Period=0.23’’

Period=0.23’’

θ=0.08’’

preliminary

H-Source Size>
1pixel=2.5um

Period17

2D Image was obtained

Gratingx2
d=9.6um, f=0.2

CMOS 2.5mmpix
GMAX0505

Ex=12.4keV, z=867cm
0.23”

0.23”

200m

z=8.67m

0.08’’
preliminary

18

“Experimental” Simulation of Two Sources
z=92cm, Rotate the Optical Bench
Real Observations of a 8GeV Jet on the Earthφ=•2.16”Merge Event Data

φ19

z=0.92m 光学台の向きを変えてデータ取得
イベントデータをマージ=2個の天体の観測模擬
φH=0.45”, φV=0.0”

φH=0.0”, φV=0.432”

φH=0.72”, φV=0.0”

φH=0.0”, φV=0.756”•2.16”

イベントデータをマージ

φV φH
20

MIXIM is scalable in unit no and in d&z
Collimator
Mask

Grating
Active Shield（Scintillator）~30mm

Wire MarkCMOS Pixel Dete.
Power Supply
APD

OpticalBlocking Filter

HeadMIXIM UNIT

Driver &Data
Processor

300mm
z~0.5m-100mCPU

pitch
openfraction
distance

Stack21Ｇｒａｔｉｎｇ
Ｐｉｔｃｈｄ（ｍ）

102

102

100

100

10-2

10-2

10-410-4q10-6 （arcsec）

10-6
10-8 -2
10ImageProfile
Width01021041061081010101210

10-8 f=0.2z(m)MIXIM-S (Small)
z=50cmθ=0.4’’

d=5mm,f=0.2
Y-modules
X-modules-P (Parasite) -Z (Zoom)
z=10m
θ=0.09’’z=10~100m
θ=0.1’’~0.01’’

d=22mm, f=0.2

d=71mm,f=0.1-L (Large/LISA)
z=2.5x106km
θ=3marcsec

d=35cm, f=0.1

MirrorGrating
Main Detector

Star Tracker

MIXIMDetector224

D=0.1mm
D=1m
D=10m
D=10km
D=10000km
Naked eye
Galileo
ALMA
GRAVITY
Herschel PACS
HST
HST
Spitzer
ChandraNuStarHitomiSGD
EHTGALEXXMM
SuzakuHitomi
EAVN

Log( Anglar Resolution[arcsec])

3Suzaku2

Spitzer

Hitomi
NuStar
XMM

10HerschelChandra-1

MIXIM-S-P-2

-Z

ALMA
HST
VLT GRAVITY

-3

EAVN

-4
EHT

-5-L-6-12-10-8-6-4Log(Wavelength [m])-2023Primary Target >mCrab almost Point-like Sources
e.g. Nearby AGNs

Ryan C. Hickox and David M. Alexander
https://ned.ipac.caltech.edu/level5/March18/Hickox/
Hickox1.html

0.5uarcsec

0.5’’

@4Mpc

Everything included in this 6 decades would be target of MIXIM
24

Very Preliminary by K. Asakura

Circinus Galaxy(Sy2) Fe-Ka line simulation

Background is not included

Aeff=10 cm2 (If we get Det. Layer of 20mm, Ageo=24cm2) 、Texp～1Ms
Opening Fraction 0.5、Minimum Patter 0.2 Mask z=8.67m

Input

ＭＩＸＩＭ Obs.

25

Jets are important target, of course.
Chandra X-ray Images of M87 from Press Release 2019
(Credit: NASA/CXC/SAO/B.Sinos)

3’’3’’26

Do we need X-ray observations aroundthe Event Horizon after EHT?
• X-ray vs RadioThanks inputs from Kawashima-san, Tazaki-san• Penetration power is highest for (hard) X-rays.
• Optically thick gas in radio can be optically thin in X-rays.
• AGNs with high accretion rate (not RIAF) can be targets for X-rays but
not for radio (?).
• Inner edge of a (standard) accretion disk, which is sensitive to BH spin,
can be imaged only with X-rays (?). Coronae, too.

• (Color) Temperature of the accreting matter can be measured
only with X-rays.
• Elemental Abundance and Doppler Motion (through Fefluorescent lines) can also be measured with X-rays.
• Enough room to diffraction limit for X-rays but not so for radio.
• The event horizon was resolved in Radio but not yet in X-rays.

X-ray would be complementary to Radio, at least27

Limitations Not like Mirrors• No Collecting Power• Additional Collimator (0.1-1deg) is needed.
• Eff. Area=Geo. Area x f x Det. Efficiency• Non Xray Background will be those forconventional collimator detectors

We should consider>mCrab apparently
point-like targets withlong exposures.

• Narrow “1-period” FOV

Many Technical Issues• Attitude Determination must be better than the image resolution.
• Conventional Star Trackers are not enough.
• Techniques used in Astrometry may help.
• Common Issue for super high angular resolution instruments• Note: Attitude Control is not as severe as• X-rays through Grating goes Detector; tolerance of mm is allowed.
• Formation flight case, fuel needed to control the grating satellite orbit may
be a problem.

• Optical CMOS detection layer is currently thin, e.g. 5um.
• …..

28

MIXIM FAQ

1. Is MIXIM interferometer?

• In the sense that the Talbot Interference condition is the key. Multi slit
camera employing the Talbot interference may be appropriate.

2. What is the FOV of MIXIM.

• Folded image within the (additional) collimator is obtained. FOV is thus
0.1-1deg, while 1-folding-period is very narrow. If we use f=0.2 grating,just 5 times of q.
• One bright point-like source within 0.1-1deg FOV is expected.

3. Effective Area of several cm2 is too small, isn’t it?

• People observe >mCrab (Suzaku) >10nCrab (Chandra) sources withTelescopes with 100-1000cm2 effective area.
• For MIXIM targets >mCrab, it should be enough• cf. We roughly estimate 0.1 c/MIXIM-unit/Crab with technicalenhancement in next few years. 5 units, 5mCrab source need 0.5Ms toDetection layer→10um,
collect 103 counts.
Geo. Area of 1 CMOS→20mmx20mm
New mask with Opening fraction of 0.5 keeping image width as 0.2

4. How can you obtain 2D image? Muti-Pin-Hole?

• 1D units placed X and Y are baseline. 2D mask with larger opening isbeing designed.
29