We present the result from a comprehensive laboratory and on-sky characterization of the commercial spectrograph system consisting of a PIXIS 1300BX charge-coupled device (CCD) camera and an IsoPlane 320A spectrograph as part of the preparation of the forthcoming all-sky spectroscopic survey of nearby galaxies (A-SPEC). In the laboratory, we have quantified readout noise, dark current, gain, and full-well capacity via bias, dark, and photon transfer curve analysis at all acquisition modes. To do that, we have developed a gradient correction technique to address row-dependent signal gradients in the image, which are caused by the shutter-less condition of our CCD camera test setup. The technique successfully reproduces the values in the manufacturer specifications. We also have measured quantum efficiency exceeding 80% from 400–800 nm and ≳ 90% between 450–750 nm, with sub-second persistence decay, making it ideal for rapid, multi-object spectroscopy. Using a set of diffraction gratings (150, 300, and 600 grmm−1), we have evaluated the spatial separability of multiple spectra and spectral resolution. We have conducted a test observation with this spectrograph system at the Seoul National University Astronomical Observatory (SAO) 1 m telescope and successfully demonstrated its capability of multi-object spectroscopy with moderate resolution of R ≈ 600–2600. We release all Python codes for the test and recipes to facilitate further instrument evaluations.

Introduction
Instruments
    CCD
    Optical Test Bench
    Spectrograph and Optical Fiber
    Instrument Control Software
Characterization of the PIXIS 1300BX
    Bias
        Gradient Effect Correction
        Readout Noise and Gradient Noise
        Bias Level Time Variability
    Dark
        Dark Current
        Internal Pattern Noise
    Photon Transfer Curve
    Linearity
    Quantum Efficiency
    Charge Persistence
Characterization of the IsoPlane 320A Spectrograph
    Spatial Separability of Multi Spectra
    Spectral Resolution
ON-SKY Tests
    Observations with SAO 1 m Telescope
    Spectroscopic Calibration
Discussion
Conclusion
Code Availability
Acknowledgments
References
Gradient Noise
Photon Transfer Curve
Linearity Curve

• Jiwon Jang(Astronomy Program, Department of Physics and Astronomy, Seoul National University, Seoul 08826, Republic of Korea)
• Hyeonguk Bahk(Astronomy Program, Department of Physics and Astronomy, Seoul National University, Seoul 08826, Republic of Korea)
• Ho Seong Hwang(Astronomy Program, Department of Physics and Astronomy, Seoul National University, Seoul 08826, Republic of Korea, SNU Astronomy Research Center, Seoul National University, Seoul 08826, Republic of Korea) Corresponding author
• Dongkok Kim(Astronomy Program, Department of Physics and Astronomy, Seoul National University, Seoul 08826, Republic of Korea, Institute for Data Innovation in Science, Seoul National University, Seoul 08826, Republic of Korea)
• Changsu Choi(SPEX Inc., R&D Center, Cheongju-si, Chungcheongbuk-do, 28165, Republic of Korea)
• Haeun Chung(University of Arizona, Steward Observatory, Tucson, AZ 85721, USA)
• Jae-Woo Kim(Korea Astronomy and Space Science Institute, Daejeon 34055, Republic of Korea)