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Charge exchange emission is known to provide a key diagnostic to theinterface between hot and cold matter in many astrophysical environments. Mostof the recent charge exchange studies focus on its emission in the X-ray band,but few on the UV part, although the latter can also provide a powerful probeof the charge exchange process. An atomic calculation, as well as anapplication to observed data, are presented to explore and describe thepotential use of the UV data for the study of cosmic charge exchange. Using thenewest charge exchange model in the SPEX code v3.03, we re-analyze an archivalHubble STIS data of the central region of NGC 1275. The NGC 1275 spectrum showshints for three possible weak lines at about 1223.6~{\AA}, 1242.4~{\AA}, and1244.0~{\AA}, each with a significance of about $2-3\sigma$. The putativefeatures are best explained by charge exchange between highly ionized hydrogen,neon, and sulfur with neutral matter. The wavelengths of the charge exchangelines are found robustly with uncertainties $\leq 0.3$~{\AA}. The possiblecharge exchange emission shows a line-of-sight velocity offset of about $-3400$km s$^{-1}$ with respect to the NGC 1275 nucleus, which resembles one of theLy$\alpha$ absorbers reported in Baum et al. (2005). This indicates that thecharge exchange lines might be emitted as the same position of the absorber,which could be ascribed to outflowing gas from the nucleus.

Charge exchange in the ultraviolet: implication for interacting clouds in the core of NGC 1275