All Tables

Table 2: The ratios of the line flux of the features measured in the PHT-S spectrum over the line flux measured in the SWS spectrum LF $_{{\rm PHT-S}}$ /LF $_{{\rm SWS}}$ . The given errors are the statistical errors on the measurements.
Table 7: The mean peak wavelength $\lambda _0$ , FWHM and peak-over-continuum flux ratio of the detected features.
Table 8: The mean line-flux ratios of the examined features. Indicated in the table is the mean LF_A/LF_B of all sample stars for which both A and B were detected.
Table 9: Supposing a homogeneous distribution of the PAH molecules in a halo around the central star, with a radius of the size of the ISO-SWS beam (11 $^{\prime \prime }$ ) at the appropriate distance, the PAH particle density $\rho$ is computed based on the $L_{{\rm PAH}}/L_{{\rm uv}}$ ratio. All objects in which PAH emission is detected are adopted in this table and are listed according to decreasing PAH-over-UV luminosity.
Table 1: The sample of HAEBEs used in this study, based on Thé et al. (1994) and Malfait et al. (1998). For each object, the observed ISO spectra are given; S01 refers to SWS AOT01, P40 to PHT-S and C04 to CAM04 spectra.
Table 3: The presence of the PAH features at 3.3, 6.2, 7.7 and 8.6 micron, the NAN features at 3.4 and 3.5 micron, the 11 micron complex (COMP 11) and the amorphous 10 micron silicate feature (Si 9.7) in the spectra of the sample stars. The sources are classified in 3 groups. $\surd$ : detection; - : no detection; n.s.: no spectrum available at these wavelengths. $\surd^{ a}$ : tentative detection; $\surd^{ b}$ : tentative detection in the PHT-S spectrum; $\surd^{ c}$ : feature undetected in the SWS spectrum; $\surd^{ d}$ : feature undetected in the PHT-S spectrum (see Sect. 2.5). For the amorphous silicate feature, E stands for emission and A for absorption. BD+40 $^\circ$ 4124, R CrA and LkH $\alpha$ 224 have not been classified based on the diagram in Fig. 5, which is indicated by the question mark.
Table 4: The line fluxes LF of the IR features included in this analysis. a(-b) represents $a \times 10^{-b}$ .
Table 5: The continuum flux at the peak wavelength of the IR features included in this analysis. When the amorphous 10 micron silicate band was present, the PAH features are superimposed on the band. In this case (flagged by $^\ast$ ), the silicate feature is regarded as being part of the underlying continuum of the PAH features. Hence the indicated continuum flux of the PAH band is the flux of the silicate feature at the central wavelength of that PAH band.
Table 6: The stellar parameters for the sample sources. The distance d which we used in the analysis and spectral type (Sp. T.) are given. The visual extinction $A_{\rm V}$ , the logarithm of the effective temperature $\log T_{{\rm eff}}$ , of the stellar luminosity $\log L$ , of the stellar UV luminosity $\log L_{{\rm uv}}$ and of the observed bolometric luminosity $\log L_{{\rm bol}}$ are presented as well. The latter quantities are estimated based on the photometric measurements. Furthermore, the ratio of the IR excess luminosity over the stellar luminosity is computed. Ten of the sample sources have a ratio larger than unity, hence are not consistent with a passive reprocessing disk. The last 4 columns contain the IR excess fluxes in K (2.2 $\mu$ m), at 60, 850 and 1300 micron. $^\bigstar$ These stars are UX Orionis objects according to the definition of Dullemond et al. (2003). $^{\spadesuit }$ Probable confusion with the nearby source CrA IRS7.