Table 2
Properties derived from the IRS spectra of our ULIRGs.
| Galaxy | S Si9.7μm |
|
EW6.2/μm | |
| (a) | (b) | (c) | ||
|
|
||||
| IRAS 00199-7426 | −1.149 | 27.11 | 0.377 | |
| IRAS 01494-1845 | −1.396 | 32.95 | 0.394 | |
| IRAS Z02376-0054 | −0.697 | 16.44 | 0.332 | |
| IRAS 04114-5117 | −1.500 | 35.40 | 0.345 | |
| IRAS 06009-7716 | −1.262 | 29.78 | 0.429 | |
| IRAS F08208+3211 | −1.424 | 33.60 | 0.346 | |
| IRAS F10156+3705 | −1.072 | 25.30 | 0.659 | |
| IRAS 10565+2448 | −1.139 | 26.89 | 0.429 | |
| IRAS 12112+0305 | −1.629 | 38.43 | 0.289 | |
| IRAS 13120-5453 | −1.475 | 34.82 | 0.373 | |
| IRAS 16334+4630 | −1.367 | 32.27 | 0.349 | |
| IRAS 17208-0014 | −1.856 | 43.80 | 0.329 | |
| IRAS 19297-0406 | −1.600 | 37.77 | 0.317 | |
| IRAS 19458+0944 | −1.810 | 42.71 | 0.414 | |
| IRAS 20414-1651 | −1.705 | 40.23 | 0.423 | |
| IRAS 22491-1808 | −1.624 | 38.33 | 0.382 | |
Notes. (a) strength of the silicate absorption feature; (b) V-band optical depth computed using the ULIRG silicate model of Sirocky et al. (2008) assuming a cold dust screen; (c) We have measured the 6.2-μm PAH feature equivalent width by, firstly, fitting the continuum emission close to the feature with a linear function anchored at 5.8 and 6.6 μm. Then, we computed the feature emission by integrating the continuum-subtracted spectrum from 5.9 to 6.5 μm, and finally we divided this by the continuum emission interpolated at 6.2 μm.
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