ISO spectroscopy of circumstellar dust in 14 Herbig Ae/Be systems: Towards an understanding of dust processing

We present Infrared Space Observatory (ISO) spectra of fourteen isolated Herbig Ae/Be (HAEBE) stars, to study the characteristics of their circumstellar dust. These spectra show large star-to-star differences, in the emission features of both carbon-rich and oxygen-rich dust grains. The IR spectra were combined with photometric data ranging from the UV through the optical into the sub-mm region. We defined two key groups, based upon the spectral shape of the infrared region. The derived results can be summarized as follows: (1) the continuum of the IR to sub-mm region of all stars can be reconstructed by the sum of a power-law and a cool component, which can be represented by a black body. Possible locations for these components are an optically thick, geometrically thin disc (power-law component) and an optically thin flared region (black body): (2) all stars have a substantial amount of cold dust around them, independent of the amount of mid-IR excess they show: (3) also the near-IR excess is unrelated to the mid-IR excess, indicating different composition/location of the emitting material: (4) remarkably, some sources lack the silicate bands: (5) apart from amorphous silicates, we find evidence for crystalline silicates in several stars, some of which are new detections: (6) PAH bands are present in at least 50% of our sample, and their appearance is slightly different from PAHs in the ISM: (7) PAH bands are, with one exception, not present in sources which only show a power-law continuum in the IR: their presence is unrelated to the presence of the silicate bands: (8) the dust in HAEBE stars shows strong evidence for coagulation: this dust processing is unrelated to any of the central star properties (such as age, spectral type and activity).

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