Molecule identified to be the source of the line emission. When two lines are too close in frequencies to be separated with the WideX channel width, the secondary spectral line is indicated in parentheses.

Upper-level energy of the transition.

Size of the best fit of an elliptical Gaussian to the visibilities, see text for further details. Gaussian fits were performed on the channel showing the maximum emission (our data has a spectral resolution of 3.9 MHz ~ 2.7  km s^-1). Most lines are detected at the systemic velocity V_sys ~ 7( ± 0.5) km s^-1. Two notable lines show several blue-shifted velocity components: SiO shows emission at 7, 3, − 14.5, and − 32.5 km s^-1, while SO is detected at velocities 6.5, − 0.5, and − 14.0 km s^-1. No FWHM is indicated when the molecular emission is dominated by an outflow- or jet-like structure, as determined by a preliminary inspection of the emission maps line per line. The ^⋆ symbol indicates the presence of a secondary component to be fitted at a different position in the map. The ^⋆⋆ symbol indicates that, in addition to the component towards IRAS2A the line also traces outflow and/or complex structures at other locations in our maps.

Position angle of the elliptical Gaussian, when an elliptical Gaussian fit could be performed successfully.

Flux attributed to the best fit with a Gaussian component located at the center of the protostellar envelope.

Critical density of the transition, computed at 100 K, using the collision rates compiled in the LAMDA database when available. http://home.strw.leidenuniv.nl/~moldata/