Tracking down the origin of superbubbles and supergiant shells in the Magellanic Clouds with Minkowski tensor analysis

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Table 3

Manually determined bubble-detection parameters in the SMC.

Hα/[O III]

w		m	Line density	w′

(pc)	(px)		threshold	(pc)	(px)
22	12	0.25	10	72	40
27	15	0.25	10	90	50
36	20	0.25	12	108	60
54	30	0.3	10	180	100
72	40	0.3	10	180	100
90	50	0.3	10	270	150
108	60	0.3	10	360	200
126	70	0.3	12	450	250

[S II]

w		m	Line density	w′

(pc)	(px)		threshold	(pc)	(px)

22	12	0.25	10	72	40
27	15	0.25	10	90	50
36	20	0.25	10	108	60
54	30	0.3	10	180	100
72	40	0.3	12	180	100
90	50	0.3	12	270	150
108	60	0.3	12	360	200
126	70	0.3	12	450	250

Notes. Parameters for Hα and [O III] images are given in the upper table and those for the [S II] image in the lower table. w and w′ refer to the smoothing window diameter of the original Minkowski map and the map at a larger scale.

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