Warm Water Vapor around Sagittarius B2

Several condensations heated externally by nearby hot stars are present in the Sgr B2 region for which H 2 O far-IR lines are expected to probe only an external low-density and high temperature section. Millimeter-wave lines can penetrate deeper into them (higher densities and lower T k ). We have conducted a study combining H 2 O lines in both spectral regions using the ISO (far-IR lines) and the IRAM 30 m telescope (183 GHz line). The far-IR H 2 O lines, seen in absorption, are optically thick. They form in the outermost gas in front of the far-IR continuum sources, probing a maximum visual extinction of ~5-10 mag. IR photons from the dust play a dominant role in their excitation. We conclude, based on observations of the CO J = 7-6 line at 806.65 GHz, and the lack of emission from the far-IR CO lines, that the gas density has to be below ~10 4 cm -3 . Using the gas kinetic temperature and density derived from OH, CO, and other molecular species, we derive a water column density of (9 ± 3) × 10 16 cm -2 in the absorbing gas, implying an abundance of ≃(1-2) × 10 -5 in this region. The resulting relatively low H 2 O/OH abundance ratio, ≃2-4, is a signature of UV photon-dominated surface layers traced by far-IR observations. As a consequence, the temperature of the absorbing gas is high, T k ≃ 300-500 K, which allows very efficient neutral-neutral reactions producing H 2 O and OH. Finally, the 183.31 GHz data allow one to trace the inner, denser ( n (H 2 ) ≥ 10 5 -10 6 cm -3 ), and colder ( T k ~ 40 K) gas. The emission is very strong toward the cores with an estimated water vapor abundance of a few × 10 -7 . There is also moderate extended emission around Sgr B2 main condensations, in agreement with the water vapor abundance derived from far-IR H 2 O lines.