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Table 3.

Dust morphology, extension, and mass for the H I-rich and H I-poor galaxies.

Gal Dist. log10Reff q HI-Typec Dust morphology
 Dust radius
[Mpc] [arcsec] − − SL07–T01 K11 This work [arcsec] [Reff] [Kpc]
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11)
NGC 0661 30.6 1.12 0.69 Poor − N N 0 0.0 0.0
NGC 0770 36.7 0.94 0.71 Poor − N D 5 0.6 0.9
NGC 2549 12.3 1.28 0.31 Poor −N N N 0 0.0 0.0
NGC 2577 30.8 1.15 0.59 Poor − N Ir 14 1.0 2.1
NGC 2592 25 1.09 0.79 Poor −D N N 0 0.0 0.0
NGC 2594 35.1 0.82 0.68 Rich − N D 10 1.5 1.7
NGC 2679 31.1 1.35 0.93 Poor − N N 0 0.0 0.0
NGC 2685 16.7 1.41 0.6 Richc − F S 100 3.9 8.1
NGC 2764 39.6 1.09 0.51 Richc − FB S 35 2.8 6.7
NGC 2852 28.5 0.85 0.86 Poor − N R 12 1.7 1.7
NGC 2859 27 1.43 0.85 Rich − N S 22 0.8 2.9
NGC 2950 14.5 1.19 0.59 Poor N–N N N 0 0.0 0.0
NGC 3098 23 1.12 0.23 Poor − N D+ 50 3.8 5.6
NGC 3230 40.8 1.26 0.39 Poor − N N 0 0.0 0.0
NGC 3245 20.3 1.40 0.54 Poorc − N Ir 15 0.6 1.5
NGC 3248 24.6 1.20 0.6 Poor − N D 5 0.3 0.6
NGC 3301 22.8 1.30 0.31 Poor − N Ir 11 0.6 1.2
NGC 3377 10.9 1.55 0.67 Poor l,0.26-F1 N Ir 19 0.5 1.0
NGC 3400 24.7 1.23 0.56 Poor − N N 0 0.0 0.0
NGC 3414 24.5 1.38 0.78 Rich S,0.15-F1 N S 30 1.3 3.6
NGC 3458 30.9 1.06 0.71 Poor − N N 0 0.0 0.0
NGC 3522 25.5 1.01 0.52 Rich − N Ir 8 0.8 1.0
NGC 3605 20.1 1.23 0.6 Poor − N R 7 0.4 0.7
NGC 3610 20.8 1.20 0.81 Poor N N N 10 0.6 1.0
NGC 3613 28.3 1.42 0.54 Poor −N N N 0 0.0 0.0
NGC 3619 26.8 1.42 0.91 Richc − FBR S 40 1.5 5.2
NGC 3626 19.5 1.41 0.67 Richc − D S 30 1.2 2.8
NGC 3648 31.9 1.12 0.56 Poor − N N 0 0.0 0.0
NGC 3658 32.7 1.28 0.84 Poor − N N 0 0.0 0.0
NGC 3665 33.1 1.49 0.78 Poorc − D R 18 0.6 2.9
NGC 3674 33.4 1.05 0.36 Poor − N N 0 0.0 0.0
NGC 3757 22.6 0.95 0.85 Poor − N N 0 0.0 0.0
NGC 3796 22.7 1.06 0.6 Poor − N Ir 7 0.6 0.8
NGC 3838 23.5 1.04 0.44 Rich − N Ir 9 0.8 1.0
NGC 3941 11.9 1.40 0.75 Rich − N Ir 26 1.0 1.5
NGC 3945 23.2 1.45 0.65 Rich i,x, FBR S 60 2.1 6.8
NGC 3998 13.7 1.30 0.78 Rich il,0.43 N Ir 35 1.8 2.3
NGC 4036 24.6 1.46 0.4 Richc il,x F S 30 1.0 3.6
NGC 4078 38.1 0.92 0.44 Poor − N D 8 1.0 1.5
NGC 4203 14.7 1.47 0.89 Richc sl,0.23 N S 50 1.7 3.6
NGC 4278 15.6 1.50 0.91 Rich i,x N Ir 30 0.9 2.3
NGC 4283 15.3 1.09 0.96 Poorc − N D 8 0.7 0.6
NGC 5173 38.4 1.01 0.87 Richc −F3 B Ir 23 2.2 4.3
NGC 5273 16.1 1.57 0.84 Poorc sl,0.14 N Ir 18 0.5 1.4
NGC 5308 31.5 1.25 0.2 Poor N–N N D+ 50 2.8 7.6
NGC 5322 30.3 1.60 0.64 Poor − N N 0 0.0 0.0
NGC 5342 35.5 0.97 0.46 Poor − N D 18 1.9 3.1
NGC 5473 33.2 1.32 0.79 Poor − N N 0 0.0 0.0
NGC 5485 25.2 1.45 0.74 Poor − D R 25 0.9 3.1
NGC 5500 31.7 1.18 0.8 Poor − N N 0 0.0 0.0
NGC 5582 27.7 1.44 0.65 Rich − N D 8 0.3 1.1
NGC 5611 24.5 1.00 0.45 Poor − N D 6 0.6 0.7
NGC 5631 27 1.32 0.93 Rich − D S 35 1.7 4.6
NGC 6547 40.8 1.06 0.33 Poor − N D+ 25 2.2 4.9
NGC 6548 22.4 1.35 0.89 Poor − N R 12 0.5 1.3
NGC 6798 37.5 1.23 0.53 Richc − N S 30 1.8 5.5
NGC 7457 12.9 1.56 0.53 Poor N N D 15 0.4 0.9
PGC 050395 37.2 1.04 0.73 Poor − N N 0 0.0 0.0
UGC 04551 28 1.03 0.39 Poor −N N Ir 10 0.9 1.4
UGC 06176 40.1 1.03 0.51 Richc − F S 31 2.9 6.0
UGC 08876 33.9 0.93 0.37 Poor − N R 12 1.4 2.0
UGC 09519 27.6 0.87 0.75 Richc − F Ir 20 2.7 2.7

Notes. Column (1): the name is the principal designation from LEDA (Paturel et al. 2003). Column (2): distance in Mpc (Cappellari et al. 2011a). Column (3): projected half-light effective radius (Cappellari et al. 2011a). Column (4): the ratio of the minor axis to the major axis obtained from the ellipticity value (Krajnović et al. 2011). Column (5): H I content of the galaxy (Serra et al. 2012). The c sign indicates CO detection (Young et al. 2011). Columns (6−7): labels used to define the dust morphology in the previous studies: Simões Lopes et al. (2007) and Tran et al. (2001) (6); Krajnović et al. (2011) (7). If the size of the dust structure is given in the previous studies, we give this value next to the label. Column (8): labels used to define the dust morphologies in this study. Columns (9)−(11): dust radius measured in this study in the units of arcsec, effective radius, and Kpc, respectively. Column (12): estimated dust masses from the total optical extinction (A(g′)). Column (13): dust masses derived from SED fits by using far-IR data (Kokusho et al. 2019). Comments. − Labels of the dust morphological classes, D: dusty disc; Ir: irregular dust; R: dusty ring; S: spiral-shaped structure; N: no-dust structure; D+: almost edge-on dusty disc. Labels used in the previous studies are different than our classes: F1: filamentary low; F3: filamentary high; l: dust lane or filament.

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