Spectra of the H₂O 1₁₁ − 0₀₀ (bottom), HO 1₁₁ − 0₀₀ (second from bottom), H₂O 2₁₂–1₀₁ (third from bottom) and H₂O 2₀₂–1₁₁ (top) lines toward IRAS 05358. The vertical scale is T_mb in K, and the dashed line denotes the systemic velocity determined from ground-based observations. The spectra have been shifted vertically for clarity.

As Fig. B.1, toward IRAS 16272.

As Fig. B.1, toward NGC 6334I(N).

As Fig. B.1, toward W43 MM1.

As Fig. B.1, toward DR21(OH).

As Fig. B.1, toward W3 IRS5.

As Fig. B.1, toward IRAS 18089.

As Fig. B.1, toward W33A. The emission/absorption feature near 0 km s^-1 in the 1669 GHz spectrum is the H₂O 1661 GHz line from the other sideband.

As Fig. B.1, toward IRAS 18151.

As Fig. B.1, toward AFGL 2591. The emission feature near +18 km s^-1 in the 1669 GHz spectrum is the H₂O 1661 GHz line from the other sideband.

As Fig. B.1, toward G 327.

As Fig. B.1, toward NGC 6334I.

As Fig. B.1, toward G29.96.

As Fig. B.1, toward G31.41.

As Fig. B.1, toward G5.89. The emission feature near +90 km s^-1 in the HO spectrum is the ¹³CO 10–9 line.

As Fig. B.1, toward G10.47.

As Fig. B.1, toward G34.26.

As Fig. B.1, toward W51e.

As Fig. B.1, toward NGC 7538 IRS1.

Continuum model for IRAS 05358. Top left: spectral energy distribution. Top right: submillimeter image with 3σ contour marked in white and useable map sectors marked in black. Bottom left: temperature and density structure as a function of radius. Bottom right: submillimeter emission profiles. The numbers in the top left panel are the modeled envelope mass, the modeled luminosity, the adopted envelope size and the adopted distance.

As Fig. C.1, for IRAS 16272.

As Fig. C.1, for NGC 6334I(N).

As Fig. C.1, for W43-MM1.

As Fig. C.1, for DR21(OH).

As Fig. C.1, for W3 IRS5.

As Fig. C.1, for IRAS 18089.

As Fig. C.1, for W33A.

As Fig. C.1, for IRAS 18151.

As Fig. C.1, for AFGL 2591.

As Fig. C.1, for G327–0.6.

As Fig. C.1, for NGC 6334I.

As Fig. C.1, for G29.96.

As Fig. C.1, for G31.41.

As Fig. C.1, for G5.89.

As Fig. C.1, for G10.47.

As Fig. C.1, for G34.26.

As Fig. C.1, for W51e.

As Fig. C.1, for NGC 7538 IRS1.

Observed line fluxes (positive: emission) or absorbances (negative: absorption) versus bolometric luminosity L of the source (top), versus envelope mass M (middle), and versus the ratio L/M (bottom). Open squares: mid-IR-quiet HMPOs; filled squares: mid-IR-bright HMPOs; triangles: hot molecular cores; circles: ultracompact Hii regions. Uncertainties in line fluxes are ≈10%, while the typical uncertainty of masses, luminosities and L/M ratios is a factor of 2.

As Fig. D.1, for the narrow outflow component.

As Fig. D.1, for the broad outflow component.

Line width of the narrow outflow component versus bolometric luminosity L of the source (top), versus envelope mass M (middle), and versus the ratio L/M (bottom). The error bar denotes the typical uncertainty in mass, luminosity, and L/M ratio; the uncertainty in line width is smaller than the symbol size.

As Fig. D.4, for the broad outflow component.