Details

Autor(en) / Beteiligte

• Ryabukhina, O L
• Kirsanova, M S
• Henkel, C
• Wiebe, D S

Titel

Star formation time-scale in the molecular filament WB 673

Ist Teil von

• Monthly notices of the Royal Astronomical Society, 2022-11, Vol.517 (4), p.4669-4678

Erscheinungsjahr

2022

Link zum Volltext

Quelle

EZB Free E-Journals

Beschreibungen/Notizen

• ABSTRACT We present the observations of ammonia emission lines toward the interstellar filament WB 673 hosting the dense clumps WB 673, WB 668, S233-IR, and G173.57+2.43. LTE analysis of the lines allows us to estimate gas kinetic temperature (≲30K in all the clumps), number density (7–17 × 103 cm−3), and ammonia column density (≈1–1.5 × 1015 cm−2) in the dense clumps. We find signatures of collapse in WB 673 and presence of compact spatially unresolved dense clumps in S233-IR. We reconstruct 1D density and temperature distributions in the clumps and estimate their ages using astrochemical modelling. Considering CO, CS, NH3, and N2H+ molecules (plus HCN and HNC for WB 673), we find a chemical age of tchem = 1–3 × 105 yrs, providing the best agreement between the simulated and observed column densities in all the clumps. Therefore, we consider tchem as the chemical age of the entire filament. A long preceding low-density stage of gas accumulation in the astrochemical model would break the agreement between the simulated and observed column densities. We suggest that rapid star formation over a ∼105 yrs time-scale take place in the filament.