LEGO - II. A 3mm molecular line study covering 100 pc of one of the most actively star-forming portions within the Milky Way disc
Journal article, 2020
The current generation of (sub)mm-telescopes has allowed molecular line emission to become a major tool for studying the physical, kinematic, and chemical properties of extragalactic systems, yet exploiting these observations requires a detailed understanding of where emission lines originate within the Milky Way. In this paper, we present 60'' (similar to 3pc) resolution observations of many 3mm-band molecular lines across a large map of the W49 massive star-forming region (similar to 100x100pc at 11kpc), which were taken as part of the 'LEGO' IRAM-30m large project. We find that the spatial extent or brightness of the molecular line transitions are not well correlated with their critical densities, highlighting abundance and optical depth must be considered when estimating line emission characteristics. We explore how the total emission and emission efficiency (i.e. line brightness per H-2 column density) of the line emission vary as a function of molecular hydrogen column density and dust temperature. We find that there is not a single region of this parameter space responsible for the brightest and most efficiently emitting gas for all species. For example, we find that the HCN transition shows high emission efficiency at high column density (10(22)cm(-2)) and moderate temperatures (35K), whilst e.g. N2H+ emits most efficiently towards lower temperatures (10(22)cm(-2); <20K). We determine XCO(1-0)similar to 0.3 x 10(20)cm(-2)(Kkms(-1))(-1), and alpha(HCN(1-0))similar to 30M(circle dot)(Kkms(-1)pc(2))(-1), which both differ significantly from the commonly adopted values. In all, these results suggest caution should be taken when interpreting molecular line emission.
stars: formation
galaxies: star formation
ISM: molecules
galaxies: ISM
ISM: clouds
galaxies: evolution
Author
A. T. Barnes
University of Bonn
J. Kauffmann
Massachusetts Institute of Technology (MIT)
F. Bigiel
University of Bonn
N. Brinkmann
Max Planck Society
D. Colombo
Max Planck Society
A. E. Guzman
National Institutes of Natural Sciences
W. J. Kim
Institut de Radioastronomie Millimétrique (IRAM)
L. Szucs
Max Planck Society
V Wakelam
University of Bordeaux
Susanne Aalto
Chalmers, Space, Earth and Environment, Astronomy and Plasmaphysics
T. Albertsson
Max Planck Society
N. J. Evans
The University of Texas at Austin
S. C. O. Glover
Heidelberg University
P. F. Goldsmith
California Institute of Technology (Caltech)
C. Kramer
Institut de Radioastronomie Millimétrique (IRAM)
K. Menten
Max Planck Society
Y. Nishimura
University of Tokyo
National Astronomical Observatory of Japan
S. Viti
University College London (UCL)
Y. Watanabe
Shibaura Institute of Technology
A. Weiss
Max Planck Society
M. Wienen
Max Planck Society
University of Exeter
H. Wiesemeyer
Max Planck Society
F. Wyrowski
Max Planck Society
Monthly Notices of the Royal Astronomical Society
0035-8711 (ISSN) 1365-2966 (eISSN)
Vol. 497 2 1972-2001Subject Categories
Astronomy, Astrophysics and Cosmology
Atom and Molecular Physics and Optics
Condensed Matter Physics
DOI
10.1093/mnras/staa1814