2008/08/28 by L. Uscanga, Lucero Uscanga, Y. Gómez +9 · 34 citations
Physics and Astronomy · #Astro and Planetary Science #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Classical mechanics #Galaxy #Geometry #Kinematics #Line (geometry) #Line-of-sight #Maser #Nebula #Physics #Planetary nebula #Position angle #RADIUS #Ring (chemistry) #Rotation (mathematics) #Stars #Stellar, planetary, and galactic studies #Torus #astro-ph
paper · pdf · doi:10.1111/j.1365-2966.2008.13815.x
published in Monthly Notices of the Royal Astronomical Society 390(3), 1127-1132 (Oxford University Press) · 7 pages, 4 figures, 2 tables. Accepted by MNRAS
arxiv created 2008/08/28 · openalex publication_date 2008/09/24 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
We have studied the kinematics traced by the water masers located at the centre of the planetary nebula (PN) K3–35, using data from previous Very Large Array (VLA) observations. An analysis of the spatial distribution and line-of-sight velocities of the maser spots allows us to identify typical patterns of a rotating and expanding ring in the position–velocity diagrams, according to our kinematical model. We find that the distribution of the masers is compatible with tracing a circular ring with a ≃0.021-arcsec (≃100-au) radius, observed with an inclination angle of 55° with respect to the line of sight. We derive expansion and rotation velocities of 1.4 and 3.1 km s−1, respectively. The orientation of the ring, projected on the plane of the sky, at position angle (PA) ≃ 158°, is almost orthogonal to the direction of the innermost region of the jet observed in K3–35, suggesting the presence of a disc or torus that may be related to the collimation of the outflow.