Table 1.
Properties of the targets.
| Name | z | Spatial | τ9.8 μm | EW (6.2/3.3) | Cont (3 μm/5 μm) | EW (12.7/11.3) |
|---|---|---|---|---|---|---|
| scale | ||||||
| (pc arcsec−1) | ||||||
| VV 114-NE | 0.0200 | 421 | 5.3 | 18.3 ± 0.9 | 0.146 ± 0.004 | 0.527 ± 0.038 |
| VV 114-S2 | 0.0200 | 421 | 6.6 | 19.1 ± 1.0 | 0.044 ± 0.002 | … |
| IRAS 05189-2524 | 0.0441 | 898 | 1.9 | 18.1 ± 0.9 | 0.469 ± 0.014 | 2.372 ± 0.176 |
| IRAS 07251-0248-E | 0.0878 | 1700 | 7.0 | 0.06 ± 0.01 | 0.064 ± 0.002 | 0.024 ± 0.002 |
| IRAS 08572+3915-NW | 0.0582 | 1180 | 6.1 | … | 0.102 ± 0.003 | 0.048 ± 0.003 |
| IRAS 09111-1007-W | 0.0541 | 1110 | 2.8 | 20.5 ± 1.2 | 0.531 ± 0.016 | 0.612 ± 0.043 |
| NGC 3256-N | 0.0094 | 193 | 1.1 | 84.6 ± 4.2 | 0.459 ± 0.011 | 0.868 ± 0.062 |
| NGC 3256-S | 0.0094 | 193 | 4.7 | 8.8 ± 0.6 | 0.007 ± 0.002 | 0.523 ± 0.037 |
| IRAS 13120-5453 | 0.0308 | 650 | 2.8 | 20.3 ± 1.0 | 0.280 ± 0.008 | 1.056 ± 0.074 |
| IRAS 14348-1447-NE | 0.0823 | 1610 | 4.2 | 81.7 ± 4.3 | 0.128 ± 0.004 | 0.463 ± 0.032 |
| IRAS 14348-1447-SW | 0.0823 | 1610 | 5.2 | 12.6 ± 0.8 | 0.094 ± 0.003 | 0.162 ± 0.01 |
| Arp 220-W | 0.0184 | 394 | 6.3 | 8.7 ± 0.4 | 0.199 ± 0.006 | 0.060 ± 0.001 |
| Arp 220-E | 0.0184 | 394 | 7.0 | 41.9 ± 2.2 | 0.098 ± 0.003 | 0.054 ± 0.001 |
| II Zw 096-D1 | 0.0362 | 783 | 2.3 | 8.0 ± 0.5 | 0.153 ± 0.004 | … |
| IRAS 22491-1808-E | 0.0778 | 1500 | 5.8 | 14.9 ± 0.7 | 0.130 ± 0.004 | 0.678 ± 0.048 |
| SF average from NGC 7469 | 0.0163 | 349 | 1.3 | 78.61 ± 2.87 | 0.677 ± 0.091 | 0.803 ± 0.181 |
| Circumnuclear region of NGC 3256 | 0.0094 | 193 | 2.0 | 76.72 ± 4.60 | 0.481 ± 0.015 | 0.690 ± 0.048 |
Notes. The redshift, and spatial scale were taken from the NASA/IPAC Extragalactic Database (NED). τ9.8 μm corresponds to the silicate strength from Donnan et al. (2024a). Given that the IR emission of VV 114-S2 is not detected at λ> 10 μm, the τ9.8 μm was derived from τ6.0 μm reported in González-Alfonso et al. (2024) by using the dust model used in Efstathiou & Rowan-Robinson (1995). The PAH EW and continuum ratios were derived in this work (see Section 5). The EW(12.7/11.3) values were derived using the IR fitting tool described in Donnan et al. (2024a). The luminosity distance and spatial scale used in this work were calculated using a cosmology with H0 = 70 km s−1 Mpc−1, Ωm = 0.3, and ΩΛ = 0.7.
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