Searching for proto-planets with MUSE | Astronomy & Astrophysics (A&A)

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Table 3

Noise fitting results of the target sample.

Name	c_{H α}	α_{H α}	σ_{bg, H α}	c_λ	α_λ	σ_bg,λ
PDS70	1.90 ± 0.56	0.50 ± 0.02	116 ± 12	2.37 ± 0.55	0.48 ± 0.02	128 ± 7
J1850-3147	7.43 ± 2.05	0.47 ± 0.02	872 ± 49	4.10 ± 1.03	0.51 ± 0.02	899 ± 21
V1094 Sco	0.08 ± 0.03	0.70 ± 0.03	61 ± 2	1.28 ± 0.22	0.48 ± 0.02	61 ± 2
V1094 Sco^(a)	0.56 ± 0.17	0.60 ± 0.3	96 ± 5	1.26 ± 0.21	0.48 ± 0.02	61 ± 2
HD 100546	0.07 ± 0.06	0.70 ± 0.05	2362 ± 1747	7.06 ± 1.70	0.50 ± 0.02	4651 ± 116
HD 163296	0.14 ± 0.06	0.63 ± 0.03	462 ± 558	1.96 ± 0.49	0.54 ± 0.02	1856 ± 43

Notes. We adopt the same notations as in Eqs. (2) and (3), where photon noise σ_photon is written as (c) and background noise is σ_bg. Unless otherwise noted, the data was processed with standard HRSDI described in Sect. 3.1. ^(a) The data was processed in modified HRSDI (see Sect. 4 for details).

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