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 Chandra If we have a diffraction limit X-ray telescope with 1m diameter, the resolution is better than that of VLBI.

What is the problem? Requirement of Small-scale Roughness : several Å Requirement of Large-scale Figure Error: ～ 1nm Easy Impossible (1) optical monitoring of the optics (2) adaptive optics system We are trying to overcome this difficulty by applying two ideas

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 Primary Mirror D=80mm F=2000mm Mo/Si Paraboloide Opt-X Separation Filter Wave Front Sensor Optical Source Deformable Mirror X-ray Optical Light 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 Wave Front Sensor Laser source with pin hole

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. Zr 150nm 85%

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.