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Table 6.

Summary of the time-dependent behaviour of each maser association in NGC6334I between 2014.7 and 2016.1 compared to predictions of the shock types and incident energy components.

Association Line area trend (a) Velocity spread trend Shock type (b) Incident energy components (c)
CM2-W1 Flare then drop Monotonic decrease J-type Thermal, infrared
CM2-W2 Flare then elevated Monotonic increase C-type Thermal, infrared, high-energy
MM1-W1 Monotonic decrease Flare then drop C-type Thermal, infrared
UCHII-W1 Flare then drop Monotonic decrease J-type Thermal, infrared, high-energy?
UCHII-W2 Monotonic decrease Monotonic decrease J-type Thermal, infrared, high-energy?
UCHII-W3 Flare then drop Monotonic decrease J-type Thermal, infrared, high-energy

Notes.

(a)

From Figure 4.

(b)

For CM2-W2 the estimate of the shock type is from considering the proper motions (Section 3.3) and the 321 GHz to 22 GHz ratio (Section 4.1.2). For the other associations, the shock type prediction is only based on proper motions.

(c)

Based on the arguments from Section 4.1.1. Whether or not the high-energy components are incident on UCHII-W1 and W2 is dependent on whether there is a cavity between MM1B and these associations.

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