Open Access

Table C.1

Optimal parameters for PSF subtraction techniques and RSM for each cluster center.

Parameters Center 1 Center 2 Center 3 Center 4 Center 5 Center 6
APCA components 20 14 18 8 7 12
APCA segments 4 3 3 3 3 4
APCA FOV rotation 0.42 0.29 0.26 0.31 0.5 0.76
NMF components 9 10 10 22 11 6
LOCI tolerance 0.0038 0.0016 0.0012 0.0057 0.0096 0.002
LOCI FOV rotation 0.49 0.14 0.48 0.1 0.13 0.73
FM KLIP components 9 19 8 12 5 5
FM KLIP FOV rotation 0.51 0.27 0.27 0.34 0.25 0.81
FM LOCI tolerance 0.0042 0.0074 0.0072 0.0073 0.0099 0.0016
FM LOCI FOV rotation 0.11 0.13 0.13 0.11 0.2 0.61
APCA δ 5 5 5 5 5 5
NMF δ 5 5 5 5 5 5
LOCI δ 5 5 5 5 5 5
FM KLIP δ 5 5 5 5 5 5
FM LOCI δ 5 5 5 5 5 5
APCA crop size 4 4 4 4 4 4
NMF crop size 4 4 4 4 4 4
LOCI crop size 4 4 4 4 4 4
FM KLIP crop size 7 7 7 7 7 7
FM LOCI crop size 7 7 7 7 7 7
APCA variance SM ST SM SM SM FR
NMF variance SM SM SM SM SM SM
LOCI variance FR ST ST SM SM ST
FM KLIP variance FR ST ST SM ST SM
FM LOCI variance SM SM ST ST ST ST

Notes. The RSM parameters include the planetary flux multiplicative factor (δ), defined as a multiple of the standard deviation, the crop size, and the variance term used to determine the noise estimation region within the annulus. The noise estimation methods are denoted as follows: “SM” (Segment with mask-based estimation), “ST” (Spatio-Temporal estimation), and “FR” (Frame-based estimation) (for further details, see Dahlqvist et al. 2021a).

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