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

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Table 2

Manually determined bubble detection parameters in the LMC.

Hα/[O III]

w		m	Line density	w′

(pc)	(px)		threshold	(pc)	(px)
29	12	0.25	23	97	40
26	15	0.25	24	121	50
48	20	0.25	20	145	60
73	30	0.3	16	242	100
97	40	0.3	17	242	100
121	50	0.3	16	364	150
145	60	0.3	17	485	200
170	70	0.3	24	606	250

[S II]

w		m	Line density	w′

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

29	12	0.25	21	97	40
26	15	0.25	22	121	50
48	20	0.25	18	145	60
73	30	0.3	14	242	100
97	40	0.3	15	242	100
121	50	0.3	14	364	150
145	60	0.3	15	485	200
179	70	0.3	20	606	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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