2013A&A...552A.123B

G29.96-0.02 is a high-mass star-forming cloud observed at 70, 160, 250, 350, and 500µm as part of the Herschel survey of the Galactic plane (Hi-GAL) during the science demonstration phase. We wish to conduct a far-infrared study of the sources associated with this star-forming region by estimating their physical properties and evolutionary stage, and investigating the clump mass function, the star formation efficiency and rate in the cloud. We have identified the Hi-GAL sources associated with the cloud, searched for possible counterparts at centimeter and infrared wavelengths, fitted their spectral energy distribution and estimated their physical parameters. A total of 198 sources have been detected in all 5 Hi-GAL bands, 117 of which are associated with 24µm emission and 87 of which are not associated with 24µm emission. We called the former sources 24µm-bright and the latter ones 24µm-dark. The [70-160] color of the 24µm-dark sources is smaller than that of the 24µm-bright ones. The 24µm-dark sources have lower L_bol and L_bol/M_env than the 24µm-bright ones for similar M_env, which suggests that they are in an earlier evolutionary phase. The G29-SFR cloud is associated with 10 NVSS sources and with extended centimeter continuum emission well correlated with the 70µm emission. Most of the NVSS sources appear to be early B or late O-type stars. The most massive and luminous Hi-GAL sources in the cloud are located close to the G29-UC region, which suggests that there is a privileged area for massive star formation toward the center of the G29-SFR cloud. Almost all the Hi-GAL sources have masses well above the Jeans mass but only 5% have masses above the virial mass, which indicates that most of the sources are stable against gravitational collapse. The sources with M_env>M_virial and that should be undergoing collapse and forming stars are preferentially located at ≲4' of the G29-UC region, which is the most luminous source in the cloud. The overall SFE of the G29-SFR cloud ranges from 0.7 to 5%, and the SFR ranges from 0.001 to 0.008M_☉/yr, consistent with the values estimated for Galactic HII regions. The mass spectrum of the sources with masses above 300M_☉, well above the completeness limit, can be well-fitted with a power law of slope α=2.15±0.30, consistent with the values obtained for the whole l=30°, associated with high-mass star formation, and l=59°, associated with low- to intermediate-mass star formation, Hi-GAL SDP fields.