All Tables

Table 1: The log of the ISO observations of Mkn 297. The nine columns list the TDT number (a unique identifier for an ISO observation), the AOT number (which identifies the observing mode used), the filter label, the wavelength range ( $\Delta \lambda$ ), the reference wavelength of the filter where appropriate, the duration of the measurement (including both the on- and off-source measurements), the field-of-view of the instrument in the configuration employed, the positional offset of the background measurement(s) with respect to the target reference position, and any additional notes.
Table 2: The ISOCAM flux densities for MIR clumps in Mkn 297. The photometry was performed before deconvolution and is accurate to about $\pm$ 15%.
Table 3: IRAS flux densities for Mkn 297 (from Sanders et al. 2003). The four columns list the filter used, the wavelength range, the reference wavelength for the filter and the flux density measured.
Table 4: PHT-SL fluxes for Mkn 297. The columns give, respectively, the line identification, the wavelength range, and the integrated line-flux and the integrated line-flux scaled to the full ISOCAM footprint, as described in Sect. 2.4.
Table 5: LWS line fluxes for Mkn 297. The three columns give the line identification, the wavelength and the line-flux respectively.
Table 6: Flux densities measured with LWS, binned to yield a single number per LWS detector.
Table 7: Total infrared luminosity and dust component masses for Mkn 297. The total FIR luminosity of $9.7\times~10^{10}$ $L_{\odot }$ places this galaxy right on the threshold of LIRG status.
Table 8: A comparison of the properties the hidden sources (h.s.) in four systems. Column 3 lists the total 15 $\mu$ m emission from the host galaxy in each case.