                !   "  " # ! !   $#   " %          !!"#$%  & ’  (&) *  !! ( +, -, ##$##  ./ *  - 0)  !! + ./&   1& !23#$%  ’ 4/ * 4*  1/ - 3! ’/,/  -, #3#2"$  Received July 23, 2007, Revised October 5, 2007 5     *& *  /  / 67(418 * // -/ / /  (’  9.-  )  /)     * )  :   4   *&  7(41  )   9.- * &   / / *  9.-  :3! ; / * *  / *    *  * - &&  *   )  *  < %% - *  *&    /     / 5     / *   )  * & $’()*+$( Recently, in the design of submillimeter and farinfrared wavelength (30  1000 "m) focal plane array, a combination of a large field of view and a high spatial resolution becomes more important for astronomical observations in order to carry them out more effectively. This requirement leads to development of larger format 2dimensional (2D) array detectors. Many researchers so far have made many efforts to realize such large format 2D array detectors based on not only conventional photoconductors and semiconductor bolometers 14 , but also high sensitive superconducting