Large-Scale Mapping Observations of DCN and DCO+^+ toward Orion KL

We present emission maps (1.5'$\times$1.5' scale, corresponding to 0.18 pc) of the DCN ($J=2-1$) and DCO$^+$ ($J=2-1$) lines in the 2 mm band toward the Orion KL region obtained with the 2 mm receiver system named B4R installed on the Large Millimeter Telescope (LMT). The DCN emission shows a peak at the Orion KL hot core position, whereas no DCO$^+$ emission has been detected there. The DCO$^+$ emission shows enhancement at the west side of the hot core, which is well shielded from the UV radiation from OB massive stars in the Trapezium cluster. We have derived the abundance ratio of DCN/DCO$^+$ at three representative positions where both species have been detected. The gas components with $V_{\rm {LSR}} \approx 7.5-8.7$ km/s are associated with low abundance ratios of $\sim4-6$, whereas much higher abundance ratios ($\sim22-30$) are derived for the gas components with $V_{\rm {LSR}} \approx 9.2-11.6$ km/s. We have compared the observed abundance ratio to our chemical models and found that the observed differences in the DCN/DCO$^+$ abundance ratios are explained by different densities.Comment: Accepted by The Astrophysical Journal, 13 pages, 5 figures, 5 table

Large-scale Mapping Observations of DCN and DCO+ toward Orion KL

We present emission maps ( 1\buildrel{\,\prime}\over{.} 5\,\times \,1\buildrel{\,\prime}\over{.} 5 scale, corresponding to 0.18 pc) of the DCN ( J = 2 − 1) and DCO ^+ ( J = 2 − 1) lines in the 2 mm band toward the Orion KL region obtained with the 2 mm receiver system named B4R installed on the Large Millimeter Telescope. The DCN emission shows a peak at the Orion KL hot core position, whereas no DCO ^+ emission has been detected there. The DCO ^+ emission shows enhancement at the west side of the hot core, which is well shielded from the UV radiation from OB massive stars in the Trapezium cluster. We have derived the abundance ratio of DCN/DCO ^+ at three representative positions where both species have been detected. The gas components with V _LSR ≈ 7.5–8.7 km s ^−1 are associated with low abundance ratios of ∼4–6, whereas much higher abundance ratios (∼22–30) are derived for the gas components with V _LSR ≈ 9.2–11.6 km s ^−1 . We have compared the observed abundance ratio to our chemical models and found that the observed differences in the DCN/DCO ^+ abundance ratios are explained by different densities