All Tables

Table 1: The sample of HAEBEs used in this analysis, based on Thé et al. (1994) and Malfait et al. (1998). For each object, the available optical spectra are indicated. Furthermore, the SIMBAD values for right ascension (RA) and declination (Dec) are given, as well as the date, start time and integration time T of the observation.
Table 2: The non-color-corrected IRAS [12]-[60] color and the near-to-mid IR luminosity ratio $L({\rm NIR})/L({\rm IR})$ of the sample sources.
Table 3: The different categories of H $\alpha$ profiles versus the types of [O I]profiles. The entries of the table are the number of stars belonging to the corresponding category. U: undetected feature, E: pure-emission profile, A: 6300 Å region rich in photospheric absorption lines, S: single-peaked profile, D: double-peaked profile, P: P Cyg-like profile, inv. P: inversed P Cyg-like profile.
Table 4: The [O I]parameters for each sample source. The objects are listed according to their IR-SED classification. The distance to the source, the effective temperature, UV luminosity and bolometric (= integrated observed) luminosity are given. References for the first two values can be found in Table 6 of AV04, unless otherwise indicated: ^A de Zeeuw et al. (1999); ^B Finkenzeller (1985); ^C Gray & Corbally (1993); ^D Gray & Corbally (1998); ^E Houk (1978); ^F Mora et al. (2001); ^G Vieira et al. (2003); ^H van den Ancker et al. (1998). The type of [O I] 6300 Å emission profile observed in each object has been indicated; E: pure-emission profile, A: 6300 Å region rich in photospheric absorption lines, U: undetected feature (upper limit). n.s.: no spectrum available. The typical errors on the FWHM and centroid position are $\pm$ 8 and $\pm$ 15 ${\rm km}~{\rm s}^{-1}$ respectively. The thirth column contains the stellar radial velocity employed in this study. This value is estimated from the available spectra, unless otherwise indicated: ^a Arce & Goodman (2002); ^b Arellano Ferro & Giridhar (2003); ^c Barbier-Brossat & Figon (2000); ^d Dunkin et al. (1997a); ^e Piétu et al. (2003); ^f Reipurth et al. (1996); ^g Yonekura et al. (1997, based on CO lines). $^\dagger$ Based on Ca II lines. $\circlearrowright$ Average of radial velocities of stars in the same field (radius $\sim$ 2 $^\prime$ ). The last two columns of the table give the type and EW of the observed H $\alpha$ profile; S: single-peaked; D: double-peaked; P: P Cygni-like; inv. P: inversed P Cyg-like. When no spectrum was available, literature values were used: ^h Arellano Ferro & Giridhar (2003); ⁱ de Winter & Thé (1990); ^j Dunkin et al. (1997a); ^k Dunkin et al. (1997b); ^l Finkenzeller & Mundt (1984); ^m Merín et al. (2004); ⁿ Pérez & Grady (1997).