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We report the discovery of (N-14)H3(3, 3) maser emission toward the DR 21(OH) star-forming region. This maser emission is spatially and spectrally coincident with CH3OH maser emission. Given the position of these (N-14)H3 and CH3OH masers relative to the observed outflow emission in DR 21(OH), along with the recent observation that thermal (N-14)H3(3, 3) emission traces outflows, we conclude that (N-14)H3 and CH3OH masers are produced within shocked molecular outflows. The sensitivity of the (N-14)H3(3, 3) maser emission to the ortho-H2/para-H2 ratio has allowed us to derive an upper limit of 106 yr to the age of the cloud which gives rise to the (N-14)H3(3, 3) maser emission.
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Mangum et al. (1994) studied this question.
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