Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 500, Issue 3, Pages 3064-3082Publisher
OXFORD UNIV PRESS
DOI: 10.1093/mnras/staa2369
Keywords
surveys; ISM: structure; Galaxy: kinematics and dynamics; radio lines: ISM
Categories
Funding
- CEA/Marie Sklodowska-Curie Enhanced Eurotalents fellowship
- Royal Society University Research Fellowship [URF/R1/191609]
- CONICYT [Basal AFB-170002]
- European Research Council [CSF-648505, 818940]
- Deutsche Forschungsgemeinschaft (DFG) via Sonderforschungsbereich (SFB) 881 The MilkyWay System
- Collaborative Research Council 956 Conditions and impact of star formation
- European Union [796461]
- Atacama Pathfinder Experiment (APEX) [092.F-9315, 193.C0584]
- DFG
- Marie Curie Actions (MSCA) [796461] Funding Source: Marie Curie Actions (MSCA)
- STFC [ST/S00033X/1] Funding Source: UKRI
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The SEDIGISM survey utilizes the APEX telescope to map the structure, excitation, and dynamics of the interstellar medium, providing insights into the large-scale distribution of cold molecular gas in the Milky Way. Results show that approximately 60% of the molecular gas is associated with the spiral arms, with 13CO emission concentrated in a small number of specific complexes rather than evenly distributed along the arms.
The SEDIGISM (Structure, Excitation and Dynamics of the Inner Galactic InterstellarMedium) survey used the APEX telescope to map 84 deg(2) of the Galactic plane between l = -60 degrees and +31 degrees in several molecular transitions, including (CO)-C-13(2 - 1) and (CO)-O-18(2 - 1), thus probing the moderately dense (similar to 10(3) cm(-3)) component of the interstellar medium. With an angular resolution of 30 arcsec and a typical 1 sigma sensitivity of 0.8-1.0K at 0.25 km s(-1) velocity resolution, it gives access to a wide range of structures, from individual star-forming clumps to giant molecular clouds and complexes. The coverage includes a good fraction of the first and fourth Galactic quadrants, allowing us to constrain the large-scale distribution of cold molecular gas in the inner Galaxy. In this paper, we provide an updated overview of the full survey and the data reduction procedures used. We also assess the quality of these data and describe the data products that are being made publicly available as part of this First Data Release (DR1). We present integrated maps and position-velocity maps of the molecular gas and use these to investigate the correlation between the molecular gas and the large-scale structural features of the Milky Way such as the spiral arms, Galactic bar and Galactic Centre. We find that approximately 60 per cent of the molecular gas is associated with the spiral arms and these appear as strong intensity peaks in the derived Galactocentric distribution. We also find strong peaks in intensity at specific longitudes that correspond to the Galactic Centre and well-known star-forming complexes, revealing that the 13CO emission is concentrated in a small number of complexes rather than evenly distributed along spiral arms.
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