ALMA-IMF — Draconitic Research

Abstract

We characterize kinematic processes in the G012.80 protocluster. We primarily focused on the N 2 H + (1-0) emission to trace the dense and cold gas. Additionally, we used complementary lines such as DCN(3-2), H41α, C 18 O(2-1), and SiO(5-4), as well as continuum maps. We performed a N 2 H + 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 in G012, which we named R1 and R2. The line-mass profiles follow λ(ω) = 5660 M ⊙ pc -1 (ω/pc) 0.30 for R1 and λ(ω) = 6943 M ⊙ pc -1 (ω/pc) 0.20 for R2. This is much larger than profiles of typical low-mass filaments. R1 and R2 show disparate position-velocity (PV) features. R1 exhibits a transverse velocity gradient of 10.4 km s -1 pc -1 and a few dense cores. This velocity gradient is interpreted with a simple rotation toy model when combined with the line-mass profile, and it corresponds to a rotational timescale of ∼0.1 Myr. In contrast, R2 exhibits compact velocity structures (∆V < 2 km s -1 ), likely due to collapse, as evidenced by the comparatively large number of massive cores and protostellar outflows. R2 is forming prestellar and protostellar cores at a rate of ∼ 55.3 M ⊙ Myr -1 , with an efficiency similar to the Orion integral shaped filament (ISF). The R1 filament, in contrast, lacks protostellar cores and only contains a few prestellar cores, resulting in an estimated star formation rate of ∼4.2 M ⊙ Myr -1 , which is lower by more than an order of magnitude than that of R2. Combining gas kinematics, core incidence, and the line-mass profiles, we suggest that R1 is younger and still rotates, while R2 has evolved to collapse with a higher star formation rate. G012 thus hosts filaments at different evolutionary stages.

Cite

BibTeX RIS

BibTeX

@article{salinas2026almaimf,
  title = {{ALMA-IMF}},
  author = {J Salinas and A M Stutz and R H Álvarez-Gutiérrez and N A Sandoval-Garrido and F Louvet and R Galván-Madrid and F Motte and M Armante and T Csengeri and J Braine and A Ginsburg and M Valeille-Manet and L Bronfman and P Sanhueza and D Díaz and G Busquet and A Koley and M Bonfand and M Fernández-López and A Gusdorf and N Castro-Toledo and R Veyry and G Bernal-Mesina},
  journal = {Astronomy \& Astrophysics - A\&A},
  year = {2026},
  month = sep,
  doi = {10.1051/0004-6361/202557551},
  url = {https://hal.science/hal-05759483v1},
  note = {CC BY 4.0},
}

RIS

TY  - JOUR
TI  - ALMA-IMF
AU  - J Salinas
AU  - A M Stutz
AU  - R H Álvarez-Gutiérrez
AU  - N A Sandoval-Garrido
AU  - F Louvet
AU  - R Galván-Madrid
AU  - F Motte
AU  - M Armante
AU  - T Csengeri
AU  - J Braine
AU  - A Ginsburg
AU  - M Valeille-Manet
AU  - L Bronfman
AU  - P Sanhueza
AU  - D Díaz
AU  - G Busquet
AU  - A Koley
AU  - M Bonfand
AU  - M Fernández-López
AU  - A Gusdorf
AU  - N Castro-Toledo
AU  - R Veyry
AU  - G Bernal-Mesina
PY  - 2026
DA  - 2026/09/22
JO  - Astronomy & Astrophysics - A&A
DO  - 10.1051/0004-6361/202557551
UR  - https://hal.science/hal-05759483v1
AB  - We characterize kinematic processes in the G012.80 protocluster. We primarily focused on the N 2 H + (1-0) emission to trace the dense and cold gas. Additionally, we used complementary lines such as DCN(3-2), H41α, C 18 O(2-1), and SiO(5-4), as well as continuum maps. We performed a N 2 H + 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 in G012, which we named R1 and R2. The line-mass profiles follow λ(ω) = 5660 M ⊙ pc -1 (ω/pc) 0.30 for R1 and λ(ω) = 6943 M ⊙ pc -1 (ω/pc) 0.20 for R2. This is much larger than profiles of typical low-mass filaments. R1 and R2 show disparate position-velocity (PV) features. R1 exhibits a transverse velocity gradient of 10.4 km s -1 pc -1 and a few dense cores. This velocity gradient is interpreted with a simple rotation toy model when combined with the line-mass profile, and it corresponds to a rotational timescale of ∼0.1 Myr. In contrast, R2 exhibits compact velocity structures (∆V < 2 km s -1 ), likely due to collapse, as evidenced by the comparatively large number of massive cores and protostellar outflows. R2 is forming prestellar and protostellar cores at a rate of ∼ 55.3 M ⊙ Myr -1 , with an efficiency similar to the Orion integral shaped filament (ISF). The R1 filament, in contrast, lacks protostellar cores and only contains a few prestellar cores, resulting in an estimated star formation rate of ∼4.2 M ⊙ Myr -1 , which is lower by more than an order of magnitude than that of R2. Combining gas kinematics, core incidence, and the line-mass profiles, we suggest that R1 is younger and still rotates, while R2 has evolved to collapse with a higher star formation rate. G012 thus hosts filaments at different evolutionary stages.
SN  - 0004-6361
SN  - 1432-0746
ER  -