The Chang’E-7 spacecraft is scheduled to be landed in the Aitken Basin region of the lunar south pole to conduct comprehensive exploration and research on the lunar surface environment. As one of the main detectors onboard the Chang’E-7 spacecraft, a lunar dust detector is developed for in-situ measurements of naturally suspended dust in the polar region, key parameters such as the particle size, velocity, and cumulative mass flux will be obtained. To achieve high-precision scientific detection, systematic ground calibration experiments were conducted. For particle size calibration, a single-particle free-fall method combined with an equivalent test scheme using neutral density filters was employed, achieving coverage of the particle size range from 1 µm to 5000 µm. Experimental results demonstrate that the particle size retrieval error does not exceed 17%. Velocity calibration was performed by measuring the time-of-flight of free-falling particles from different heights, yielding a velocity measurement error within 13%. For mass flux calibration, the solution titration method was used to obtain the sensitivity of the Quartz Crystal Microbalances, with sensitivities in three orthogonal directions all on the order of 10^–9 g·Hz^–1·cm^–2 and exhibiting good linearity. Furthermore, temperature-frequency correction curves were established to support the normalization of in-orbit data. The calibration results indicate that the performance indicators of the dust detector meet the requirements for detection in the extreme environment of the lunar south pole. The established calibration methods and retrieval models provide a reliable foundation for the interpretation of subsequent in-orbit scientific data.

The Chang’E-7 mission will deploy China’s first independently developed lunar seismograph at the Moon’s south pole to record ground motions generated by moonquakes and meteoroid impacts. The instrument is designed for an eight-year operation lifetime aimed at characterizing the seismic activity and shallow interior structure of the Moon. To ensure measurement accuracy and long-term operational stability under the extreme conditions of the lunar environment, it is essential to establish a systematic calibration methodology. This will guarantee that the instrument’s key technical parameters and calibration indicators meet the requirements for scientific exploration and data inversion. Based on the technical criteria for ground-based seismograph network integration, and considering performance specifications such as bandwidth, dynamic range, and magnitude range, this paper proposes a comprehensive ground calibration test plan covering critical indicators, including amplitude-frequency response, sensitivity and sensitivity error, self-noise levels and measurement range. Furthermore, in accordance with the operational requirements during the lunar surface phase, an autonomous in-situ calibration scheme has been designed, along with a proposed manual source calibration method on the lunar surface. This study establishes a comprehensive calibration framework for the functionality and performance of the lunar seismograph, providing systematic procedures for performance testing and evaluation throughout all mission phases—from ground validation to in-situ operation on the lunar surface. The proposed framework lays an essential foundation for acquiring high-precision lunar seismic data and conducting subsequent scientific analyses.

The Chang’E-7 mission carries a Lunar Penetrating Radar (LPR) for investigating lunar shallow subsurface structures. To ensure the validity of the acquired data and improve the accuracy and consistency of its interpretation, this study presents a comprehensive calibration framework suitable for space-grade penetrating radar systems, incorporating full-system gain calibration and system transfer function calibration, among others. Applying this methodology, the lunar radar system was rigorously calibrated, clarifying the optimal parameter configuration for its in-orbit operation. Under this parameter setting, all performance metrics of the radar system meet the design requirements: the system gains of the Low-Frequency (LF) and High-Frequency (HF) channels are 171.02 dB and 169.70 dB, respectively, fulfilling the detection depth requirements of 400 m and 40 m. The acquired Time-Varying Gain (TVG) curve and system transfer function, validated through simulated lunar regolith experiments, can provide effective calibration baselines for scientific data obtained during lunar surface exploration. This calibration scheme can serve as a technical reference for the calibration of radar systems in future deep-space exploration missions.

The Chang’E-7 orbiter is expected to carry the Wide-band InfraRed Imaging Spectrometer (WIRIS), which will acquire high spectral resolution images and thermal emission data of the lunar surface across a broad spectral range from the visible to longwave infrared (0.45～10 µm). These data will support scientific investigations into lunar surface mineral composition, thermal environment, and water/hydroxyl detection. Compared to previous lunar orbital hyperspectral instruments, WIRIS enhances quantitative retrieval capabilities for key spectral features such as the Christiansen Feature (CF) of silicate minerals and molecular water. Building upon the design of the Tianwen-1 Mars Mineralogical Spectrometer, WIRIS extends its spectral coverage into the mid- to long-wave infrared range (3.3～10 μm), and incorporates simultaneous temperature measurements to reduce thermal correction uncertainties in the 3 μm water/hydroxyl absorption region. This study addresses the quantitative calibration requirements of the newly extended spectral range by proposing spectral, radiometric, and geometric calibration methods tailored for the mid- to long-wave infrared bands. Based on calibration experiments, the sources of error and associated uncertainties are analyzed. The results provide essential methodological and technical support for accurate physical parameter retrieval and scientific application of WIRIS mid- to long-wave infrared data.

After the Chang’E-7 lunar microwave imaging radar in the fourth phase of the Lunar Exploration Project is put into on-orbit operation in the future, calibration devices will not be deployed on the lunar surface, making on-orbit External calibration impossible. To ensure the acquisition of high-precision lunar surface image data, a ground calibration method is proposed. This method combines the internal calibration of the radar system with the performance calibration in the inner field. During ground testing, the internal calibration accuracy and the consistency of internal calibration channels are obtained by measuring the temperature characteristics of the internal calibration network under a full-temperature environment. The internal calibration constants are acquired in an anechoic chamber. By constructing a wireless transceiver environment in the inner field with the help of the anechoic chamber, the absolute transceiver gains and the stability of the transceiver channels of the system are accurately calibrated. The basic data obtained through ground calibration can be used for the calibration of indicators such as on-orbit internal calibration constants, absolute and relative radiation accuracy, and polarization channel consistency, providing guarantee for high-resolution lunar surface exploration.

The Moon provides a unique and advantageous platform for astronomical observations, particularly in the visible and ultraviolet wavelength ranges, owing to its extremely tenuous exosphere, the absence of atmospheric turbulence, and a stable surface environment. These characteristics enable long-duration, continuous observations free from atmospheric interference. As one of the international payloads aboard the Chang’E-7 mission, the International Lunar Observatory Camera (ILO-C) project aims to exploit these advantages to observe the Milky Way and the broader universe from a distinctive lunar perspective. In addition to its scientific objectives, the project offers unique value for astronomy education and serves as a technology demonstration for future lunar-based astronomical observatories. The ILO-C camera will be mounted on the +y panel of the Chang’E-7 lander and will experience multiple mission phases, including cruise, lunar orbit, and surface operations. This paper systematically investigates the scientific calibration workflow for the ILO-C across these mission phases, with particular emphasis on fundamental calibration, color calibration, and flux calibration, and further presents observational and calibration pathways for cross-validation. The quality of the project’s scientific output will largely depend on the optimized implementation of these calibration schemes. Ideally, in-flight activation and observations are expected to be achieved, allowing coverage of a broader sky area and enabling cross-comparison with observations from other space-based and ground-based astronomical facilities.

The Kp index is a parameter designed to indicate the level of global geomagnetic disturbances originating from the interaction of the solar wind with the magnetosphere. The index is defined at 3-hour intervals and has 28 levels. Kp is a global version of the local K index, which was conceived by Bartels and is commonly used in scientific research of the solar-terrestrial relationship. The continuity of the index over 50 year makes it particularly valuable in studies of solar-cycle variations and other long-term effects on interplanetary and magnetospheric phenomena. For example, Kp has been used in studies of solar wind shock waves, the interplanetary magnetic field, plasma density variations in the magnetosphere, and magnetospheric ULF waves. In addition, the index is widely used as an input to magnetospheric/ionospheric models. For example, the plasmapause is modeled to move closer to the Earth with increasing Kp. The location of substorm injection is modeled to have a similar Kp dependence. The magnetic field model of Tsyganenko has an explicit Kp dependence, and the magnetotail becomes more stretched for higher Kp. These models are used both in scientific research and in monitoring and predicting space weather. In 2011, the National Space Science Center of the Chinese Academy of Sciences established the Chinese Academy of Sciences Space Environment Monitoring Network, which included Mohe, Beijing, Langfang, Sanya, and Fuke stations. A geomagnetic Kp_est index, which can effectively identify the day-to-day variation characteristics of the geomagnetic regular daily variation, reflect the seasonal and local time effects of geomagnetic disturbances, and is suitable for the distribution characteristics of China’s geomagnetic observatory network, has been developed through the integration and processing of the H-component monitoring data from fluxgate magnetometers at these five geomagnetic observatory stations. This dataset contains the geomagnetic Kp_est indices for the five geomagnetic observatory stations from 2022 to 2024. It addresses the current situation where the official Kp index is released with a two-week delay, failing to meet operational requirements, and can provide data support for space weather forecasting services.

The Muon Telescope at Siziwang Station in Inner Mongolia is used to detect the secondary cosmic ray muons reaching the ground. The Muon Telescope began construction in November 2019, was completed in April 2023, and produced scientific data. The muon telescope consists of a scintillator observation stack, an electronics recorder, a monitoring platform, and a power supply. The scintillator observation stack is composed of 48 detector units, divided into upper and lower layers with 24 units in each layer, arranged in a 6×4 array. In each detector unit, the plastic scintillator has dimensions of 50 cm × 50 cm × 5 cm. The distance between the upper and lower layers is 89 cm. A 5cm-thick layer of lead bricks is laid between the upper and lower layers to filter out low-energy cosmic rays and low-energy particles in the surrounding environment. The detectors have a total area of 6 m². Muon signals generated by the 48 detector units of the Muon Telescope are processed through front-end circuits for amplification, discrimination, and shaping, then sent to the FPGA logic circuit for directional coincidence calculation. This produces raw muon counts in 15 directions. After undergoing barometric correction calculation, a dataset of corrected muon counts in 15 directions is formed, with a temporal resolution of 1 hour. The count rate in the vertical direction is the highest, with the 1-hour count rate being around 600000 counts and the relative statistical error approximately 0.13%. The muon data can sensitively reflect diurnal variations, long-term variations of cosmic rays, and short-term Forbush decrease perturbations induced by coronal mass ejections. Spanning from May 2023 to April 2025, this dataset covers the high-activity phase of the 25th solar activity cycle. It provides valuable data resources for research on solar eruptions, their interplanetary disturbance propagation, and geomagnetic response processes, while also supporting space weather early warning efforts.