Duration and properties of the embedded phase of star formation in 37 nearby galaxies from PHANGS-JWST

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Table B.1.

Main input parameters used in the analysis for galaxies ordered by increasing Hubble morphological T-types.

Galaxy	t_CO^a	l_ap, min^b	l_ap, max^c	N_pix^d	ΔF_CO^e	δF_CO^f	ΔF₂₁^g	δF₂₁^h	n_λⁱ	N $_{mask}^{21}$ $_{\mathrm{mask}}^{21}$ ^j	$F_{mask}^{21}$ $F_{\mathrm{mask}}^{21}$ ^k

NGC1512	10.1 $\pm_{2.3}^{2.7}$ $\pm_{2.3}^{2.7}$	110	3000	15	1.2	0.05	2.0	0.05	11	3 (0.3%)	22.3 (12.8%)
NGC1433	17.2 $\pm_{2.5}^{2.0}$ $\pm_{2.5}^{2.0}$	109	3000	15	1.9	0.05	2.0	0.05	12	7 (1%)	22.8 (17.3%)
NGC4941	24.2 $\pm_{4.0}^{5.4}$ $\pm_{4.0}^{5.4}$	149	3000	10	2.5	0.05	1.6	0.05	12	0	-
NGC5134	12.4 $\pm_{2.4}^{2.9}$ $\pm_{2.4}^{2.9}$	123	3000	10	3.4	0.05	2.0	0.05	12	3 (1.6%)	64.8 (40.1%)
NGC4548	13.2 $\pm_{2.5}^{5.3}$ $\pm_{2.5}^{5.3}$	149	3000	8	2.5	0.05	2.5	0.05	14	0	-
NGC3507	12.1 $\pm_{1.6}^{2.5}$ $\pm_{1.6}^{2.5}$	176	7000	7	3.0	0.1	1.8	0.05	12	0	-
NGC3351	21.0 $\pm_{2.7}^{4.6}$ $\pm_{2.7}^{4.6}$	84	3000	15	1.8	0.05	2.0	0.05	12	2 (0.5%)	24.8 (11.6%)
NGC3627	13.3 $\pm_{1.8}^{2.6}$ $\pm_{1.8}^{2.6}$	121	3000	15	3.2	0.05	2.0	0.05	13	4 (2.8%)	371.5 (58.1%)
NGC6300	19.9 $\pm_{2.7}^{4.4}$ $\pm_{2.7}^{4.4}$	85	3000	15	2.2	0.05	2.2	0.15	13	2 (0.4%)	83.6 (5%)
NGC7496	16.8 $\pm_{2.9}^{9.8}$ $\pm_{2.9}^{9.8}$	168	5000	15	3.0	0.05	2.5	0.05	13	1 (0.8%)	37.1 (20.2%)
NGC1365	23.8 $\pm_{6.1}^{95.2}$ $\pm_{6.1}^{95.2}$	173	1500	20	2.7	0.05	2.0	0.05	13	4 (2.3%)	16.3 (61.4%)
NGC1097	16.1 $\pm_{2.9}^{3.2}$ $\pm_{2.9}^{3.2}$	137	3000	7	2.1	0.05	2.1	0.05	14	3 (1.1%)	45.7 (16.6%)
IC1954	12.5 $\pm_{2.2}^{3.4}$ $\pm_{2.2}^{3.4}$	131	3000	7	2.5	0.05	2.0	0.05	14	2 (1.4%)	46.2 (6.7%)
NGC4303	19.1 $\pm_{2.9}^{3.0}$ $\pm_{2.9}^{3.0}$	155	3000	15	1.6	0.05	2.5	0.05	13	7 (2.4%)	155.2 (31.6%)
NGC1566	21.9 $\pm_{3.1}^{3.3}$ $\pm_{3.1}^{3.3}$	115	3000	15	2.5	0.05	2.5	0.05	12	4 (1.4%)	272.5 (34.4%)
NGC3059	32.6 $\pm_{5.5}^{9.2}$ $\pm_{5.5}^{9.2}$	149	5000	20	3.5	0.05	2.0	0.05	10	0	-
NGC1300	12.3 $\pm_{1.1}^{1.8}$ $\pm_{1.1}^{1.8}$	122	3000	15	1.5	0.05	2.0	0.05	11	4 (2.3%)	41.3 (28.7%)
NGC4321	18.9 $\pm_{2.2}^{3.3}$ $\pm_{2.2}^{3.3}$	138	3000	15	1.6	0.05	2.0	0.05	12	3 (0.5%)	116.2 (8.7%)
NGC2090	10.3 $\pm_{1.8}^{2.0}$ $\pm_{1.8}^{2.0}$	112	3000	10	2.5	0.05	2.0	0.05	12	2 (1.1%)	22.7 (9.5%)
NGC4689	20.5 $\pm_{3.0}^{3.9}$ $\pm_{3.0}^{3.9}$	110	3000	15	3.0	0.05	2.5	0.05	13	0	-
NGC5042	12.8 $\pm_{2.1}^{3.0}$ $\pm_{2.1}^{3.0}$	133	3000	10	2.5	0.05	2.5	0.1	12	0	-
NGC5643	19.0 $\pm_{3.3}^{3.9}$ $\pm_{3.3}^{3.9}$	85	3000	15	2.5	0.1	2.5	0.1	11	0	-
NGC2835	8.0 $\pm_{1.2}^{1.4}$ $\pm_{1.2}^{1.4}$	74	3000	15	1.2	0.05	2.0	0.05	12	3 (1.1%)	134.5 (17.5%)
NGC0628	15.6 $\pm_{1.9}^{2.3}$ $\pm_{1.9}^{2.3}$	53	3000	15	1.1	0.05	2.0	0.05	13	7 (1.4%)	71.6 (46.1%)
NGC1087	15.6 $\pm_{2.8}^{3.6}$ $\pm_{2.8}^{3.6}$	143	3000	15	1.5	0.1	2.5	0.1	13	2 (1.5%)	45.6 (43.2%)
NGC3596	17.5 $\pm_{2.3}^{3.5}$ $\pm_{2.3}^{3.5}$	74	3000	4	3.5	0.1	2.0	0.05	14	0	-
NGC0685	12.9 $\pm_{2.4}^{4.4}$ $\pm_{2.4}^{4.4}$	169	3000	10	3.0	0.05	2.0	0.05	13	3 (1.6%)	10.5 (15.4%)
IC5273	12.7 $\pm_{2.8}^{3.8}$ $\pm_{2.8}^{3.8}$	153	3000	6	2.5	0.05	2.0	0.05	12	2 (1.5%)	91.0 (43.5%)
NGC4731	12.6 $\pm_{3.2}^{28.7}$ $\pm_{3.2}^{28.7}$	148	3000	5	2.5	0.05	2.5	0.156	13	2 (2.7%)	21.8 (50.2%)
NGC1385	13.3 $\pm_{2.7}^{6.7}$ $\pm_{2.7}^{6.7}$	124	3000	10	1.7	0.05	3.0	0.05	14	2 (1.1%)	230.0 (31.5%)
NGC2283	9.2 $\pm_{2.1}^{2.4}$ $\pm_{2.1}^{2.4}$	102	3000	15	1.4	0.05	2.5	0.05	13	0	-
NGC5068	11.7 $\pm_{1.4}^{2.6}$ $\pm_{1.4}^{2.6}$	32	3000	15	1.6	0.03	2.0	0.03	10	0	-
NGC4951	11.7 $\pm_{3.0}^{2.9}$ $\pm_{3.0}^{2.9}$	167	5000	10	2.4	0.05	2.0	0.05	12	2 (1.5%)	15.5 (9.7%)
NGC4540	12.9 $\pm_{3.3}^{4.7}$ $\pm_{3.3}^{4.7}$	111	3000	15	3.0	0.05	3.0	0.05	14	2 (1.5%)	39.5 (17.6%)
NGC4571	18.4 $\pm_{2.8}^{4.8}$ $\pm_{2.8}^{4.8}$	127	3000	7	3.0	0.4	2.0	0.05	12	0	-
NGC4781	7.8 $\pm_{1.1}^{1.6}$ $\pm_{1.1}^{1.6}$	99	3000	15	2.5	0.05	2.3	0.05	12	2 (1.0%)	49.4 (14.4%)
NGC4496A	15.8 $\pm_{3.0}^{3.1}$ $\pm_{3.0}^{3.1}$	117	3000	10	3.0	0.05	2.5	0.05	12	3 (1.5%)	42.5 (10.0%)

Notes.

Total cloud lifetime in Myr (reference timescale in the current study), recalculated with updated masks with respect to K22.

Minimal aperture size (in parsecs ).

Maximal aperture size (in parsecs ).

Minimal number of pixels to used in the peak identification with CLUMPFIND.

Logarithmic range below flux maximum covered by flux contour levels for molecular gas peak identification in CO maps.

Logarithmic interval between flux contour levels for molecular gas peak identification in CO maps.

Logarithmic range below flux maximum covered by flux contour levels for SFR peak identification in 21 μm maps.

Logarithmic interval between flux contour levels for SFR peak identification in 21 μm maps.

ⁱ

Softening parameters used to filter diffuse emission in both CO and 21 μm maps.

Total number of bright 21 μm peaks masked in our analysis (and fraction with respect to the total number of 21 μm peaks).

Surface brightness threshold (in MJy/sr) used to mask bright peaks (and fraction of the total 21 μm compact flux they represent).

Other parameters which are not listed here are set to the values adopted in K22 for the variables adjusted individually for each galaxy, and Kruijssen et al. (2018) for the default quantities chosen to run HEISENBERG.

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