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Context. G29.96-0.02 is a high-mass star-forming cloud observed at 70, 160,250, 350, and 500 microns as part of the Herschel survey of the Galactic Planeduring the Science Demonstration Phase. Aims. We wish to conduct a far-infraredstudy of the sources associated with this star-forming region by estimatingtheir physical properties and evolutionary stage, and investigating the clumpmass function, the star formation efficiency and rate in the cloud. Methods. Wehave identified the Hi-GAL sources associated with the cloud, searched forpossible counterparts at centimeter and infrared wavelengths, fitted theirspectral energy distribution and estimated their physical parameters. Results.A total of 198 sources have been detected in all 5 Hi-GAL bands, 117 of whichare associated with 24 microns emission and 87 of which are not associated with24 microns emission. We called the former sources 24 microns-bright and thelatter ones 24 microns-dark. The [70-160] color of the 24 microns-dark sourcesis smaller than that of the 24 microns-bright ones. The 24 microns-dark sourceshave lower L_bol and L_bol/M_env than the 24 microns-bright ones for similarM_env, which suggests that they are in an earlier evolutionary phase. TheG29-SFR cloud is associated with 10 NVSS sources and with extended centimetercontinuum emission well correlated with the 70 microns emission. Most of theNVSS sources appear to be early B or late O-type stars. The most massive andluminous 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 formationtowards the center of the G29-SFR cloud. Almost all the Hi-GAL sources havemasses well above the Jeans mass but only 5% have masses above the virial mass,which indicates that most of the sources are stable against gravitationalcollapse. The sources with M_env > M_virial and that ...

A Hi-GAL study of the high-mass star-forming region G29.96-0.02