Disk winds have been postulated as a mechanism for angular momentum release in protostellar systems for decades. HD 163296 is a Herbig Ae star surrounded by a disk and has been shown to host a... Show moreDisk winds have been postulated as a mechanism for angular momentum release in protostellar systems for decades. HD 163296 is a Herbig Ae star surrounded by a disk and has been shown to host a series of HH knots (HH 409) with bow shocks associated with the farthest knots. Here we present ALMA science verification data of CO J = 2-1 and J = 3-2 emission, which are spatially coincident with the blue shifted jet of HH knots, and offset from the disk by -18.6 km s$^{-1}$. The emission has a double corkscrew morphology and extends more than 10'' from the disk with embedded emission clumps coincident with jet knots. We interpret this double corkscrew as emission from material in a molecular disk wind, and that the compact emission near the jet knots is being heated by the jet that is moving at much higher velocities. We show that the J = 3-2 emission is likely heavily filtered by the interferometer, but the J = 2-1 emission suffers less due to the larger beam and sensitivity to larger scale structures. Excitation analysis suggests temperatures exceeding 900 K in these compact features, with the wind mass, momentum and energy being of order 10$^{-5}$ M$_{⊙}$, 10$^{-4}$ M$_{⊙}$ km s$^{-1}$ and 10$^{40}$ erg, respectively. The high mass loss rate suggests that this star is dispersing the disk faster than it is funneling mass onto the star. Show less
Context. G29.96-0.02 is a high-mass star-forming cloud observed at 70, 160, 250, 350, and 500 {$μ$}m as part of the Herschel survey of the Galactic plane (Hi-GAL) during the science demonstration... Show moreContext. G29.96-0.02 is a high-mass star-forming cloud observed at 70, 160, 250, 350, and 500 {$μ$}m as part of the Herschel survey of the Galactic plane (Hi-GAL) during the science demonstration phase. Aims: 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. Methods: 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. Results: A total of 198 sources have been detected in all 5 Hi-GAL bands, 117 of which are associated with 24 {$μ$}m emission and 87 of which are not associated with 24 {$μ$}m emission. We called the former sources 24 {$μ$}m-bright and the latter ones 24 {$μ$}m-dark. The [70-160] color of the 24 {$μ$}m-dark sources is smaller than that of the 24 {$μ$}m-bright ones. The 24 {$μ$}m-dark sources have lower L$_{bol}$ and L$_{bol}$/M$_{env}$ than the 24 {$μ$}m-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 70 {$μ$}m 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$_{env}$ {gt} M$_{virial}$ and that should be undergoing collapse and forming stars are preferentially located at {lsim}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 0.008 M$_{⊙}$ yr$^{-1}$, consistent with the values estimated for Galactic Hii regions. The mass spectrum of the sources with masses above 300 M$_{⊙}$, well above the completeness limit, can be well-fitted with a power law of slope {$α$} = 2.15 {plusmn} 0.30, consistent with the values obtained for the whole l = 30{deg}, associated with high-mass star formation, and l = 59{deg}, associated with low- to intermediate-mass star formation, Hi-GAL SDP fields. Tables 1-3 are available in electronic form at http://www.aanda.orgShow less