Filamentary structure and Keplerian rotation in the high-mass star-forming region G35.03+0.35 imaged with ALMA

摘要: Context. Theoretical scenarios propose that high-mass stars are formed by disk-mediated accretion. Aims. To test the theoretical predictions on formation of massive stars, we wish to make a thorough study at high-angular resolution structure and kinematics dust gas emission toward star-forming region G35.03+0.35, which harbors disk candidate around B-type (proto)star. Methods. We carried out ALMA Cycle 0 observations 870 μm typical high-density, molecular outflow, cloud tracers with resolutions < 0"5. Complementary Subaru COMICS 25 were trace mid-infrared this region. Results. The submillimeter continuum has revealed filamentary fragmented into six cores, called A–F. filament could be in quasi-equilibrium taking account mass per unit length filament, 200–375 M_⊙/pc, is similar critical thermally turbulently supported infinite cylinder, ~335 M_⊙/pc. average separated ~0.02 pc, have deconvolved sizes 1300–3400 AU, temperatures 35–240 K, H_2 densities >10^7 cm^(-3), masses range 1–5 M_⊙, they subcritical. Core A, associated hypercompact Hii driving source outflow observed region, most chemically rich G35.03+0.35 strong hot core such as CH_3CN. Tracers high density excitation show clear velocity gradient along major axis core, consistent rotating about outflow. PV plots SE–NW direction signatures Keplerian rotation, although infall also present, pattern an edge-on star 5–13 M_⊙. t_(ff)/t_(rot) ratio for A suggests rotates fast accreting material time settle centrifugally disk. Conclusions. one convincing examples disks (proto)stars. This supports according least would form through accretion.