The characterization of detectors installed in space- and ground-based instruments is important to evaluate the system performance. We report the development of a detector performance test system for astronomical applications using the Andor iKon M CCD camera. The performance test system consists of a light source, monochromator, integrating sphere, and power meters. We adopted the Czerny–Tuner monochromator with three ruled gratings and one mirror, which covers a spectral range of 200–9,000 nm with a spectral resolution of ~1 nm in the visible region. Various detector characteristics, such as the quantum efficiency, sensitivity, and noise, can be measured in wide wavelength ranges from the visible to mid-infrared regions. We evaluated the Korea Astronomy and Space Science Institute (KASI) detector performance test system by using the performance verification of the Andor iKon-M CCD camera. The test procedure includes measurements of the conversion gain (2.86 e−/ADU), full well capacity (130 K e−), nonlinearity, and pixel defects. We also estimated the read noise, dark current, and quantum efficiency as a function of the temperature. The lowest measured read noise is 12 e−. The dark current at 223 K was determined to be 7 e−/s/pix and its doubling temperature is 5.3°C ± 0.2°C at an activation energy of 0.6 eV. The maximum quantum efficiency at 223 K was estimated to be 93 % ± 2 %. We proved that the quantum efficiency is sensitive to the operating temperature. It varies up to 5 % in the visible region, while the variation increases to 30 % in the near-infrared region. Based on the comparison of our results with the test report by the vendor, we conclude that our performance test results are consistent with those from the vendor considering the test environment. We also confirmed that the KASI detector performance test system is reliable and our measurement method and analysis are accurate.

1. INTRODUCTION
 2. KASI DETECTOR PERFORMANCE TESTSYSTEM
 3. CHARACTERIZATION OF THE ANDORIKON-M CCD CAMERA
  3.1 Conversion Gain
  3.2 Full Well Capacity
  3.3 Nonlinearity
  3.4 Dark Current
  3.5 Read Noise
  3.6 Pixel Defects
  3.7 Quantum Efficiency
 4. DISCUSSION AND CONCLUSION
 REFERENCES

• Young Sam Yu(Korea Astronomy and Space Science Institute) Corresponding Author
• Jinsol Kim(Chungnam National University)
• Chan Park(Korea Astronomy and Space Science Institute)
• Woong-Seob Jeong(Korea Astronomy and Space Science Institute)
• Minjin Kim(Kyungbook National University)
• Seonghwan Choi(Korea Astronomy and Space Science Institute)
• Sung-Joon Park(Korea Astronomy and Space Science Institute)