Arcsecond and Sub-arcsecond Imaging with Multi Image X-ray Interferometer for (Very) Small Satellites

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Jeremy Griffin
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1 X-ray Universe July Arcsecond and Sub-arcsecond Imaging with Multi Image X-ray Interferometer for (Very) Small Satellites K. Hayashida, T. Kawabata, H. Kurubi, H. Nakajima, S. Inoue, H. Tsunemi (Osaka University)

-Instruments for X-ray Astronomy- Agree? 1.

Detectors. 2. 0.5 resolution mirror is exceptional.

Slits, Masks or Collimators are used for wide FOV surveys, in which angular

Some function in lab, but application in orbit are even more difficult.

2 -Instruments for X-ray Astronomy- Agree? 1. Telescopes are build with Grazing Incidence Mirrors with FL of 3-12m plus Pixel Detectors resolution mirror is exceptional. It is very much difficult to reproduce it now. primarily 3. Slits, Masks or Collimators are used for wide FOV surveys, in which angular resolution is limited to ~10arcminutes. 4. Interferometers have been proposed. Some function in lab, but application in orbit are even more difficult. Chandra m 0.5 Athena m NASA / SAO / CXC ESA Attempt to challenge these common sense 5 HXT on Yokoh / Mod. Collimator m 5 ISAS/JAXA 500km 0.1mas MAXIM Pathfinder NASA

3 Multi-Pinhole(Slit) Camera is the baseline haru04/e/a8ef27218dee a a431 STACK these multiple images in the analysis

4 Multi Image X-ray Interferometer/Imager Almost Parallel Beam Grating Pitch dd Image Width θθ Opening Fraction ff Distance zz 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 dd in the analysis, accurate source profile is obtained. Image Width θθ = ffff/zz = 0.4 ff 0.2 dd / zz 5μμμμ 50cccc See Hayashida+ SPIE Proc 2016 X-ray Pixel Detector (CCD/CMOS) Stack Chandra Resolution with a 50cm size satellite?

$But, in reality Diffraction is significant.$ stacked) X-ray Intensity dd=5µm ff=0.2 z=0.5m λ=0.

5 But, in reality Diffraction is significant. Simulated Image Profile with Fresnel Approximation (not stacked) X-ray Intensity dd=5µm ff=0.2 z=0.5m λ=0.115nm N=1 (Single Slit) N=2 (Double Slit) N=3 N=10 N>>1 (Grating) Position (µm) on the Detector

6 But, but, Talbot Effect can be employed Talbot Effect Parallel Light through a grating makes Self Image of the grating 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 Distance zz TT = mm dd22 λλ Plain Wave Light mm = 1 mm = 2 mm = 3 Talbot Carpet Image from Wen et al. Advances in Optics and Photonics 5, (2013) For λ=0.1nm(12kev) X-rays and a dd=5µm pitch grating, Talbot distance zz TT of mm=2 is 50cm

7 At Talbot Distance dd=5µm ff=0.2 z=0.5m λ=0.100nm (m=2) Simulated Image Profile with Fresnel Approximation (not stacked) N=1 (Single Slit) N=2 (Double Slit) N=3 N=10 Self Image N>>1 (Grating) Position (µm) on the Detector

001λλ 0 1.002λλ 0 1.003λλ 0 1.004λλ 0 1.005λλ 0 Average (0.

8 λ dependence at a fixed setup dd=5µm ff=0.2 z=0.5m (m=2) 0.995λλ λλ λλ λλ λλ 0 λλ 0 =0.1nm 1.001λλ λλ λλ λλ λλ 0 Average ( nm nm) Band width (ΔΔΔΔ/λλ) = 111 Position (µm) on the Detector

9 λ dependence at a fixed setup dd=5µm ff=0.2 z=0.5m m=2 0.95λλ λλ λλ λλ λλ 0 λλ 0 =0.1nm 1.01λλ λλ λλ λλ λλ 0 Average (0.0954nm nm) Band width (ΔΔΔΔ/λλ) = m=2 Position (µm) on the Detector

10 Another X-ray beam incidence from 0.5arcsec offset direction dd=5µm ff=0.2 z=0.5m m=2 0.95λλ λλ λλ λλ λλ 0 λλ 0 =0.1nm 1.01λλ λλ λλ λλ λλ 0 Average (0.0954nm nm) Band width (ΔΔΔΔ/λλ) = m=2 0.5 Position (µm) on the Detector

Multi Image X-ray Interferometer Module (or Mission) = MIXIM X-ray Grating with a few~10 s µm pitch and X-ray Imaging Spectrometer Select X-ray Events of which energy is

11 Multi Image X-ray Interferometer Module (or Mission) = MIXIM X-ray Grating with a few~10 s µm pitch and X-ray Imaging Spectrometer Select X-ray Events of which energy is within specific band around the Talbot condition. Band-pass ΔΔΔΔ/λλ of about 10% (for m=2; 20% for m=1) can be utilized. Wider than Si-detector energy resolution of 1~2%. Good for X-ray CCD and X-ray CMOS. Stacked Image tell us the X-ray source profile Hayashida+ SPIE Proc 2016 c.f. X-ray Talbot (-Lau) Interferometer Momose+(2003), Pfeiffer+(2006) for Phase Contrast X-ray Imaging of Light Material Figure from Hoshino KONICA MINOLTA TECHNOLOGY REPORT Vol11

$Pitch dd=4.8µm Open frac.$

12 Lab. Experiment with Spherical Wave ~1m X-ray CMOS (XRPIX2b) inside Vacuum Chamber Cooled -40degC Window=0.2mm Thick Al microfocusx-ray 60kV, 100µA, Target=W Source Size=3~5µm X-ray Grating Pitch dd=4.8µm Open frac. ff=0.5 17µm thick Au on Si 70mm XRPIX2b pixel size 30μm 152x152 pix (Tsuru+2014)

13 Lab. Experiment Result 1/2 u- Focus XRPIX Image R=42mm, 25X mag WLβ 9.8keV WLγ 11.3keV WLα 8.4keV MoKα 17.5keV Single Pixel Event Double Pixel Event R Grating 30μm/pixel XRPIX L=1040.5mm(fixed) Projection to CA-axis Stacked Profile Only Double Events(split along CA direction) are employed Projected Profile

14 Lab. Experiment Talbot Distance for a Spherical Wave Results 2/2 Projected Profile (One Part) R=42mm, Mag. =25x R=102mm,Mag.=10x R=235mm(correspond to Talbot Condition), Mag.=4.4x Stacked Profile Fractional Amplitude =0.172+/ Fractional Amplitude =0.011+/ Fractional Amplitude = / μm@XRPIX 51μm@XRPIX 21μm@XRPIX, 0.7pix micro-focus source size of 3-5um is not small enough to be regarded as a point source as illustrated in the Stacked profile.

95λλ 0 λλ 0 =0.1nm 1.05λλ 0 1.11λλ 0 1.16λλ 0 1.22λλ 0 1.

15 Near Field zz zz TT dd=25µm, ff=0.2, λ 0 =0.1nm zz=0.5m <<zz TT mm = 1 =6.25m 0.73λλ λλ λλ λλ λλ 0 λλ 0 =0.1nm 1.05λλ λλ λλ λλ λλ 0 Average 0.073nm-0.127nm) Band width (ΔΔΔΔ/λλ) = maybe more Position (µm) on the Detector

16 Very Preliminary Design zz = mmdd 2 /λλ = 50cm mm 2 θθ = ffff zz = ffff/dddd = 0.4 ff Hayashida+2016SPIE Proc. and Updates dd 5μμμμ / λλ 0.1nnnn λλ / dd 0.1nnnn 5μμμμ θθ :Image Width dd :Pitch ff :Open. Frac. zz :Distance mm :Talbot Order mm Positional Resolution of Pixel Detector is essential. Energy Range 5-20keV Grating transmission ηη gggggg at open (Si filled) part, and Detector efficiency ηη dddddd limits the range. Effective Area AA eeeeee = AA gggggg ηη gggggg ηη dddddd ff Δλλ/λλ FOV must be limited by collimators to ~1deg. 5mm pitch Collimator Grating Detector 25cm z=25cm (Active) Shield f=0.5 Background Imaging capability reduce the CXB and NXB factor of ff. Rough estimate CXB=0.2 mcrab, NXB=4mCrab Very preliminary 2 2 Gratings=micro-collimator 100µm f=0.2 z=50cm Detector (Active) Shield

17 MIXIM options Mission Size Sampler Short Tall Grande Distance zz 0.5m 0.5m 2m 10m Pitch dd 25µm 5µm 10µm 10µm Open. Frac. ff Talbot Order mm for 0.1nm X-ray (0.1) θθ Δλλ/λλ No. of X+Y unit (AAAAAAoo=10cm 2 /unit assumed) ηη dddddd at 10keV (200um Si assuemd) Effective Area (@10keV) cm 2 2.5cm 2 16cm 2 31cm 2

Targets : e.g. Structure of Relatively Bright Pointlike Sources, i.e., (SM)BH and NS Recoiled SMBH candidates HST CXO J101527.

Kim; Optical: NASA/STScI) Torus Type2 and 1 AGNs 0.2 NGC6240 4'' NASA/CXC/MPE/S.

18 Targets : e.g. Structure of Relatively Bright Pointlike Sources, i.e., (SM)BH and NS Recoiled SMBH candidates HST CXO J Chandra Binary SMBHs Chandra 10 (X-ray: NASA/CXC/NRAO/D.-C.Kim; Optical: NASA/STScI) Torus Type2 and 1 AGNs 0.2 NGC6240 4'' NASA/CXC/MPE/S.Komossa et al. NGC1068 ALMA image 1kpc Garcia-Burillo+2016

19 -Instruments for X-ray Astronomy- Agree? 1. Telescopes are build with Grazing Incidence Mirrors with FL of 3-12m plus Pixel Detectors resolution mirror is exceptional. It is very much difficult to reproduce it now. primarily 3. Slits, Masks or Collimators are used for wide FOV surveys, in which angular resolution is limited to ~10arcminutes. 4. Interferometers have been proposed. Some function in lab, but application in orbit are even more difficult. Chandra m 0.5 Athena m 5 HXT on Yokoh / Mod. Collimator m 5 ISAS/JAXA 500km 0.1mas MAXIM Pathfinder NASA / SAO / CXC ESA No, in future, with MIXIM or any other methods. NASA

Exercise 8: Interference and diffraction

$Exercise 8: Interference and diffraction$ Physics 223 Name: Exercise 8: Interference and diffraction 1. In a two-slit Young s interference experiment, the aperture (the mask with the two slits) to screen distance is 2.0 m, and a red light of wavelength