LEGO - II. A 3mm molecular line study covering 100 pc of one of the most actively star-forming portions within the Milky Way disc
Artikel i vetenskaplig tidskrift, 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.

ISM: molecules

ISM: clouds

stars: formation

galaxies: star formation

galaxies: evolution

galaxies: ISM

Författare

A. T. Barnes

Universität Bonn

J. Kauffmann

Massachusetts Institute of Technology (MIT)

F. Bigiel

Universität Bonn

N. Brinkmann

Max-Planck-Gesellschaft

D. Colombo

Max-Planck-Gesellschaft

A. E. Guzman

Natl Inst Nat Sci

W. J. Kim

Institut de Radioastronomie Millimétrique (IRAM)

L. Szucs

Max-Planck-Gesellschaft

V Wakelam

Université de Bordeaux

Susanne Aalto

Chalmers, Rymd-, geo- och miljövetenskap, Astronomi och plasmafysik

T. Albertsson

Max-Planck-Gesellschaft

N. J. Evans

The University of Texas at Austin

S. C. O. Glover

Universität Heidelberg

P. F. Goldsmith

California Institute of Technology (Caltech)

C. Kramer

Institut de Radioastronomie Millimétrique (IRAM)

K. Menten

Max-Planck-Gesellschaft

Y. Nishimura

University of Tokyo

National Astronomical Observatory of Japan

S. Viti

University College London (UCL)

Y. Watanabe

Shibaura Inst Technol

A. Weiss

Max-Planck-Gesellschaft

M. Wienen

University of Exeter

Max-Planck-Gesellschaft

H. Wiesemeyer

Max-Planck-Gesellschaft

F. Wyrowski

Max-Planck-Gesellschaft

Monthly Notices of the Royal Astronomical Society

0035-8711 (ISSN) 1365-2966 (eISSN)

Vol. 497 2 1972-2001

Ämneskategorier

Astronomi, astrofysik och kosmologi

Atom- och molekylfysik och optik

Den kondenserade materiens fysik

DOI

10.1093/mnras/staa1814

Mer information

Senast uppdaterat

2020-11-19