Sun Yat-sen University (SYSU) has a long history of astronomy education and research, founding the first astronomy department in China in 1927, building the CUHK Observatory in Yuexiu Mountain, Guangzhou in 1929, and establishing the School of Physics and Astronomy in Zhuhai Campus in 2015, with the Department of Astronomy starting to enroll undergraduate students in astronomy in 2019. The Department of Astronomy is committed to the discipline construction and scientific research in the fields of galactic cosmology, stellar and planetary physics, multi-messenger astronomy, and astronomical instrument technology. The school is building a modern astronomical observation facility that combines education and scientific research on the top of the mountain Da Nan Shan (22.344 191 N, 113.557 600 E) in the Zhuhai campus. The site has good astronomical observation conditions, with an altitude of 407 meters, annual observation days of 120 days, and a seeing range of 0.6"~2.5". The 1.2-meter telescope of Sun Yat-sen University is a multi-functional astronomical observation facility with a full-aperture 1.2-meter primary mirror, which can carry out diversified scientific observation in a full field of view of 15 degrees and achieve the construction purpose of integrating scientific research and education. A tricolour camera set will provide real-time colour information of celestial bodies to help quickly identify and classify target celestial bodies; the long-slit spectrograph can provide low-resolution (R=1 000~3 000) spectral observation capability for point sources and extended sources, helping to study the formation and evolution of galaxies, star clusters, and other targets; a fiber-fed high-resolution spectrograph will provide single-target high-resolution (R≥30 000) spectral observation capability to assist in the measurement of special astrochemical abundance and apparent velocity.The most important feature of the SYSU 1.2-meter telescope project is that integrates diversified functionalities in imaging and spectroscopic observation. It allows university teachers and students to carry out some experimental observation without the assistance of the professional staff, and can quickly and flexibly switch different observation methods, effectively meeting the requirements of education and research. An octahedral Cassegrain unit is designed to accommodate all the science instruments and their auxiliary devices. Every instrument can connect the fold Cassegrain focus by a switching mirror on the centre of the Cassegrain unit. The unit is divided to 4 layers from top to bottom, including the flange, instrument layer, electronic layer, and cable wrapper. A shield is also prepared to remove the stray light from the background. The long-slit spectrograph is composed of full dioptric lenses, which are able to fully cover all the spectrums over the science field of 5' along the slit. It can change the spectral resolution by switching the slit widths from 1" to 3", and selecting the observing band by using different grisms. Each grism has the same function, so that the dispersed beam at the central wavelength overlaps with the optical axis of the spectrograph. It results in that the instrument doesn't require optical alignment when switching the resolution or observing the band. The high-resolution spectrograph is a powerful workhorse instrument which connects the Cassegrain focus by a 25 m fiber. It adopts a standard “White Pupil” optical system to provide the required spectral resolution over the full wavelength range from 400 nm to 900 nm by using an echelle grating and a pair of cross-dispersed prisms. A 2 000×2 000 detector is used to cover all 55 orders of spectrums with similar image quality at different wavelengths. As a result of test, the mean of spectral resolution is higher than 40 000 over the full band. A calibration unit is composed of lamps, the integral sphere, and the beam projector. It is mounted on one of the instrument ports of the octahedral Cassegrain unit. The calibration unit is able to evenly illuminate a long area with a length of longer than 20 mm. The distance of 400 mm between the lenses and the illuminated area is used to turn the calibration beam to the different instruments, the high-resolution spectrograph or the long-slit spectrograph. The paper gives a detailed introduction to the development of the above spectroscopic facilities and some results of the related technical tests at the laboratory.