DoG-HiT: A novel VLBI multiscale imaging approach | Astronomy & Astrophysics (A&A)

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Table 3

Widths of DoG wavelets and their main sensitivity to the uv-coverage, i.e., which antenna pair is mainly covered by these scales.

Scale	σ₁ → σ2 (µas)	Main Sensitivity
0	0.84 → 1.69	Unresolved
1	1.69 → 3.37	Unresolved
2	3.37 → 4.23	Unresolved
3	4.23 → 5.78	PV-SMA/JCMT
4	5.78 → 6.66	Gap
5	6.66 → 7.06	AA/AP-JCMT/SMA, AA/AP-PV
6	7.06 → 12.18	AA/AP-SMT, SMT-PV, LMT-PV
7	12.18 → 14.13	AA/AP-LMT, JCMT/SMA-LMT
8	14.13 → 17.55	JCMT/SMA-SMT
9	17.55 → 33.69	Gap
10	33.69 → 39.81	LMT-SMT
11	39.81	AA-AP, JCMT-SMA

Notes. Different scales are most sensitive either to specific baselines or the gaps in the uv-coverage. The three smallest scales were added to complete the dictionary down to the pixel size and compress unresolved structures.

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