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Ultra High Precision X-ray
Telescope Project
(X-mas Project)
S. Kitamoto, T. Kohmura, N. Yamamoto, H. Saito, H.
Takano, H. Sekiguchi, K. Suga (Rikkyo Univ.) E. Miyata, K.
Hayashida (Osaka), T. Dotani, Y. Ueda, H. Kunieda (ISAS),
K. Yamashita, Y. Tawara, Y. Ogasaka, K. Tamura(Nagoya),
H. Awaki (Ehime), M. Ishida (Tokyo-Metro), T.
Mihara(Riken), S. Tashira(Saitama), M. Itoh(Kobe)
Abstract
We started development of an ultra high
precision X-ray Telescope, named X-ray
milli-arc-sec Project (X-mas Project)
in order to propose a future space mission.
Some current basic study of the telescope
will be reported.
1. Introduction
Chandra is providing us wonderful X-ray
images and we are enjoying lots of
important scientific results.
However, the current achievement of the
image quality is still far from the theoretical
diffraction limit!
Diffraction Limit
If we have a diffraction limit X-ray telescope with
1m diameter, the resolution is better than that of
VLBI.
Chandra
What is the problem?
Requirement of Small-scale
Roughness : several Å
Easy
Requirement of Large-scale
Figure Error: ～1nm
Impossible
We are trying to overcome this
difficulty by applying two ideas
(1) optical monitoring of the optics
(2) adaptive optics system
Some Technical Consideration
A normal incident telescope is easier
than the grazing incident telescope.
Possible
precision
of
the
shape
measurement is a few nm.
13.5nm band is currently best choice.
Mo/Si Multi-Layers has more than 70%
reflectivity for the normal incident mirror.

2.Design for Laboratory Experiment
Deformable
Mirror
Optical
Optical Source
Light
Primary Mirror
D=80mm
F=2000mm
Mo/Si
Paraboloide
Opt-X Separation Filter
X-ray
Wave Front Sensor
Back Illumination
CCD
Wave Front Sensor
HASO32 (Imagine Optic)


Shack-Hartmann Sensor
Micro-lens array + CCD
Testing the precision of the
wave front sensor
Installed in a clean
booth covered by a
Black Curtain
Laser source with pin hole
Wave Front Sensor
Precision of the Wave Front
Sensor
Wave front is constructed
by pin hole images
Remove the tilt and
spherical component
Calculate the residuals
and rms variation
Less than 3nm rms has
been achieved.
Deformable Mirror (DFM)
31 elements-Bimorph
piezo-electric plates


two layer piezos with the
opposite polarity.
The plate makes a
curvature of concave or
convex shape.
55mmφ effective area
Bimorph piezo-electric plates
Flat plate made by DFM
Using Zygo
Interferometer

5.26nm rms flat
plate had been
achieved.
Some examples of the deformation
Primary Mirror
Off Axis Paraboloide



D=80mm
f=2000mm
Mo/Si Multi-layers
25-50% reflectivity
The diffraction limit
is ~50 milli-arc-sec
Detector
Back-illumination CCD (HPK)


30% detection efficiency at 13.5nm
512x512 pixels
 ２４ micro-m square
Expected image size is 0.3 micro-m

We have to study a super pixel read-out
method and to have a fine pixel chip.
Opt-X Separation Filter
Zr filter has a good transmission
Now start to design
Fine polished frame
have been ordered.
 Depositing an optically
flat filter is scheduling.
 This filter will be
fabricated and evaluated
during this year.

85%
Zr 150nm
Plan
Development of position determination method of
the CCD
Development of the feed-back control system
Fabrication and Evaluation of the Opt-X separation
filter
Integration of the telescope and evaluate the
performance with optical light
Preparation of the soft X-ray source
Preparation of the vacuum experiment
Demonstration of the telescope performance with
X-rays
Plan
Propose the X-mas satellite mission in
futur
Try to challenge the shorter wave
length and larger diameter
Fukue et al.
Challenge Direct imaging of the Black Holes.