Abstract
Coronal emission lines, especially the [Fe x]λ6374 line, are now being used as tracers for intermediate mass black holes (IMBHs) in low-mass galaxies. We show that the recent discovery of [Fe x]λ6374 emission in the metal-poor starburst SDSS J094401.87-003832.1 by Reefe et al. is, in fact, a misidentified line. The line interpreted as [Fe x]λ6374 is Si ii λ6371. We caution that current and future campaigns hunting for IMBHs with the [Fe x]λ6374 line need to account for possible contamination by Si ii λ6371 emission.
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