DESHIMA (DEep Spectroscopic HIgh-z MApper) is an on-chip filter bank spectrometer that
utilizes NbTiN superconducting resonant filters.  The output signal of each filter is
read out by Microwave Kinetic Inductance Detectors (MKIDs).  The high multiplexing
capability of MKIDs enables us to realize wide-band coverage with moderate frequency
resolution.  One of the features of DESHIMA is a combination of nano-technology and
superconducting detectors, and it will lead to extended possibilities for future sub-mm
astronomical instruments.

The target frequency band of DESHIMA is 326-905 GHz with a frequency resolution of F/dF
= 500.  The first generation of DESHIMA, covering a frequency range of 326-368 GHz, is
planned to be installed on the ASTE telescope at the Atacama Desert in 2017.  The main
components of the DESHIMA instrument are 4 K cold optics cooled down by a pulse tube
cooler, MKIDs cooled down to 100 mK by an adiabatic demagnetization refrigerator (ADR),
and FFT based multi-tone readout circuits.  The design, fabrication, assembly, and cool
down test of the instrument have been successfully carried out by collaboration between
Delft University of Technology (TU Delft), Netherlands Institute for Space Research
(SRON), and the University of Tokyo.  We have also constructed a laboratory evaluation
system of the whole DESHIMA instrument at TU Delft.  Now, the characteristics of the
sub-mm filter-bank, noise of MKIDs, and throughput efficiency have been measured using
the system to prepare for the test observing campaign at the ASTE telescope.

In this talk, I would like to present the details of the DESHIMA instrument including
the filter-bank, MKIDs, cryostat, and readout electronics together with the results of
performance evaluation.