When the focal plane temperature fluctuates, dark current's magnitude and response both change; the effective area, etching process, electron transfer efficiency, and readout circuit performance of each area array detector pixel are different [16], as is the instantaneous dark current response value. In a study conducted by the Shanghai Institute of Technical Physics of the Chinese Academy of Sciences, the QWIP's dark current was greatly affected by temperature fluctuation, which led to anomalies in the detector's light field uniformity experiment [17].  
It is not possible to directly measure the time-continuous dark current response in engineering applications. It is not accurate to infer fluctuations in the dark current level by calculating the response of all pixels in the focal plane, as changes in the target's background radiation also cause the overall level to fluctuate significantly. Conventional methods of radiation calibration also make it difficult to eliminate temporal noise caused by dark current. Correction by measuring the overall temperature of the focal plane, as well as factors such as uneven temperature distribution and measurement errors, can introduce other noise. Suppressing dark current noise using a readout circuit is highly accurate [18]; however, the presence of a readout circuit increases the overall detector size and power consumption, the fabrication process is difficult, and it has not been verified in large surface array detectors at temperatures below that of liquid nitrogen. Multiple radiometric calibrations in a short period can reduce the effect of dark current noise but compresses the continuous imaging time. As a result, some momentary key image information is missed, especially during gaze-type imaging [19; 20]. Designing reference pixels such as dark pixels in the focal plane is a general method. The QWIPs in the LWIR payload of Landsat 8 and Landsat 9 have dark pixels that cannot receive external radiation and are used to monitor the dark current level in the focal plane [21; 22; 23]. However, the dark pixels' raw data are not publicly available and there is no research regarding the correction method based on the QWIP's dark pixels data. In the detection of visible light and infrared bands, there are methods such as using numerical methods for dark current correction, using devices with low dark current, suppressing dark current by lowering the cooling temperature, and changing the driving method of the detector to reduce dark current. However, none of them apply to the reduction of dark current noise.  
We propose a method to correct the temporal noise of dark currents based on setting dark pixels in the detector. We define dark pixels, describe the preparation of the QWIP used in the study, introduce the detection system's design, and analyze the method's principles. In the experiment, the method continuously acquired feature data in the laboratory and fitted the mapping relationship between dark pixels and imaging pixels using an RNN. The acquired target data and the dark pixels' response were used to obtain the dark level correction value of the imaging pixels, and the imaging pixels' response was corrected. The effectiveness of this method was verified by comparing the data's temporal noise values before and after correction.