Browsing by Author "Salinas Cornejo, Javiera Carolina"

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    N2H+ kinematics in the g012.80 protocluster: Evidence for filament rotation and evolution.
    (Universidad de Concepción, 2024) Salinas Cornejo, Javiera Carolina; Stutz, Amelia Marie
    We aim to characterize kinematic processes in the G012.80 protocluster (hereafter G012), also known as the W33 main clump. We principally use N2H+ (1−0) emission to trace the dense and cold gas in G012. Additionally, we reviewed complementary spectral lines including DCN, H41α, C18O, SiO, and continuum maps, all observations were provided by the ALMA-IMF Large Program. We perform a N2H+ hyperfine spectral line fitting to analyze multiple velocity components and extract spectral parameters. We estimated velocity gradients, column densities, and line-mass profiles for the two main filaments, R1 & R2, which show distinct position-velocity (PV) features. In the PV diagrams we observe zig-zag, twisting, and turning velocity structures pervasively in the dense gas. However, R1 exhibits a gradient feature of 10.4kms−1 pc−1, corresponding to an estimated timescale of 0.1Myr, potentially associated with filament rotation, as well as few cores above the completeness limit. In contrast, R2 exhibits compact velocity structures (∆V∼3kms−1), likely related to collapse, as evidenced by the presence of a comparatively large number of massive cores. Line-mass profiles follow λ(ω)=5660(ω/pc)0.30 for R1 and λ(ω)=6943(ω/pc)0.20 for R2, where ω is the projected radius in the plane-of-the-sky of the aligned f ilaments. R2 forms prestellar and protostellar cores at a star formation rate of SFR=55.3M⊙Myr−1, with efficiency similar to Orion ISF. In contrast, the R1 filament, which lacks protostellar cores, only contains a few cores in the prestellar phase, resulting in an SFR of 4.24M⊙ Myr−1. Considering the dense gas kinematic, core formation, and line-mass profiles difference, we propose that R1 is still rotating and younger than the R2 filament, which has evolved further, toward collapse, to a higher star formation rate. G012 thus contains massive filaments in different evolutionary stages.
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