Akademik Veri Yönetim Sistemi
Monthly Notices of the Royal Astronomical Society, cilt.548, sa.2, 2026 (SCI-Expanded, Scopus)
The supernova remnant (SNR) G25.1–2.3 was identified in the radio band during the Sino–German (Formula presented) 6 cm survey of the Galactic plane. We present a detailed investigation of the optical, H i, and CO emission towards the G25.1–2.3 to better understand its characteristics and environment. In this study, optical spectroscopic data of the remnant and its environment have been analysed for the first time, providing new insights into their emission properties. The Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST) and 1.5-m Russian–Turkish Telescope (RTT150) data show variations across the observed regions, with [S ii]/H(Formula presented) ranging from 0.16 to 0.83. We identified shock-heated gas in the northern and southern regions and several photoionized regions around the SNR based on their [S ii]/H(Formula presented) ratios derived from spectra. The [S ii](Formula presented) 6716/(Formula presented) 6731 ratio observed in the northern region suggests electron densities ((Formula presented) ) ranging from 120 to 1030 cm(Formula presented), whereas the southern regions show higher values, between 490 and 4500 cm(Formula presented). The variations in the observed H(Formula presented) /H(Formula presented) ratios indicate significant differences in extinction across the regions. H(Formula presented) images obtained using the 1-m Turkish Telescope (T100) reveal optical emission in the northern and southern, characterized by filamentary and diffuse structures. We newly found a hole-like distribution of H i, whose spatial extent is roughly consistent with the diameter of the SNR. Based on radio data, we examine the evolutionary stage of G25.1–2.3 using the surface brightness–diameter ((Formula presented) ) relation and the equipartition method.