Artículos de revistas
The SEDIGISM survey: First data release and overview of the galacti structure
Fecha
2021Registro en:
MNRAS 500, 3064–3082 (2021)
10.1093/mnras/staa2369
Autor
Schuller, F.
Urquhart, J. S.
Csengeri, T.
Colombo, D.
Duarte Cabral, A.
Mattern, M.
Ginsburg, A.
Pettitt, A. R.
Wyrowski, F.
Anderson, L.
Azagra, F.
Barnes, P.
Beltran, M.
Beuther, H.
Billington, S.
Bronfman Aguilo, Leonardo Jaime
Cesaroni, R.
Dobbs, C.
Eden, D.
Lee, M. Y.
Medina, S. N. X.
Menten, K. M.
Moore, T.
Montenegro Montes, F. M.
Ragan, S.
Rigby, A.
Riener, M.
Russeil, D.
Schisano, E.
Sánchez Monge, A.
Traficante, A.
Zavagno, A.
Agurto, C.
Bontemps, S.
Finger, R.
Giannetti, A.
González, E.
Hernández, A. K.
Henning, T.
Kainulainen, J.
Kauffmann, J.
Leurini, S.
López, S.
Mac-Auliffe, F.
Mazumdar, P.
Molinari, S.
Motte, F.
Muller, E.
Nguyen Luong, Q.
Parra, R.
Pérez Beaupuits, J. P.
Schilke, P.
Schneider, N.
Suri, S.
Testi, L.
Torstensson, K.
Veena, V. S.
Venegas, P.
Wang, K.
Wienen, M.
Institución
Resumen
The SEDIGISM (Structure, Excitation and Dynamics of the Inner Galactic InterstellarMedium) survey used the APEX telescope
to map 84 deg2 of the Galactic plane between = −60◦ and +31◦ in several molecular transitions, including 13CO(2 – 1) and
C18O(2 – 1), thus probing the moderately dense (∼103 cm−3) component of the interstellar medium.With an angular resolution
of 30 arcsec and a typical 1σ 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.