Appendix B: Notes to individual sources

A short description of the field around each IRAS source is reported in Papers I and II. Here we provide additional information found in the more recent literature:

• - IRS 63 - 6.7 GHz methanol maser emission has been searched for without result (limiting flux $\sim 5$ Jy; Van der Walt et al. 1996). It is an IRAS PSC associated with a bright-rimmed cloud found near an OB association (Sugitani & Ogura 1994).

• - IRS 13 - CS (2-1): ($T_{\rm mb}=1.33$ K; $v_{\rm LSR}$ = +9.5 km s^-1; $\Delta v = 1.9$ km s^-1; Bronfman et al. 1996). 6.7 GHz methanol maser emission has been searched for with negative results (limiting flux $\sim 5$ Jy; Van der Walt et al. 1995).

• - IRS 14 - It coincides with the sources PRH$\alpha$161/162 (Pettersson & Reipurth 1994). This source has been classified as a Herbig Ae/Be star by Thé et al. (1994) and, as such, the properties of its circumstellar envelope have been investigated by Pezzuto et al. (1997).

• - IRS 17 - Water and 6.6 GHz methanol masers were searched for (Scalise Jr. et al. 1989; Schutte et al. 1993). CS (2-1): ($T_{\rm mb}=5.28$ K; $v_{\rm LSR}$ = +3.7 km s^-1; $\Delta v = 4.3$ km s^-1; Bronfman et al. 1996).

• - IRS 18 - A 6.6 GHz methanol maser was detected at +11, +15 km s^-1 (Schutte et al. 1993).

• - IRS 19 - Selected as planetary nebula candidate and not detected at 6 cm (rms $\sim$ 1 mJy; Van de Steene & Pottasch 1993). CS (2-1): ($T_{\rm mb}=5.80$ K; $v_{\rm LSR}$ = +12.0 km s^-1; $\Delta v = 2.9$ km s^-1; Bronfman et al. 1996).

• - IRS 20 - CS (2-1): ($T_{\rm mb}=1.01$ K; $v_{\rm LSR}$ = +2.1 km s^-1; $\Delta v = 2.3$ km s^-1; Bronfman et al. 1996). 6.7 GHz methanol maser emission has been searched for with negative results (limiting flux $\sim 5$ Jy; Van der Walt et al. 1995).

• - IRS 71 - A possible H$\alpha$ star has been detected at (19.8, 18) arcsec with respect to the IRAS position (Marquez-Limon et al. 1992 - their # 29). It coincides with our # 85, a source which lies slightly below the reddening line of A0 V stars in the colour-colour diagram and exhibits a relatively small reddening ($A_V \sim 2$).