The SEDIGISM survey: Molecular cloud morphology

I. Classification and star formation^★

¹ Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
e-mail: kneralwar@mpifr-bonn.mpg.de
² School of Physics & Astronomy, Cardiff University, Queen’s building, The parade, Cardiff CF24 3AA, UK
³ Centre for Astrophysics and Planetary Science, University of Kent, Canterbury CT2 7NH, UK
⁴ Laboratoire d’Astrophysique (AIM), CEA, CNRS, Université Paris-Saclay, Université Paris Diderot, Sorbonne Paris Cité, 91191 Gif-sur-Yvette, France
⁵ Space Science Institute, 4765 Walnut St Suite B, Boulder, CO 80301, USA
⁶ School of Science and Technology, University of New England, Armidale NSW 2351, Australia
⁷ I. Physikalisches Institut, Universität zu Köln, Zülpicher Strasse 77, 50937 Cologne, Germany
⁸ Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany
⁹ Astrophysics Research Institute, Liverpool John Moores University, IC2, Liverpool Science Park, 146 Brownlow Hill, Liverpool L3 5RF, UK
¹⁰ Laboratoire d’astrophysique de Bordeaux, CNRS, Univ. Bordeaux, B18N, allée Geoffroy Saint-Hilaire, 33615 Pessac, France
¹¹ School of Physics and Astronomy, University of Exeter, Stocker Road, Exeter EX4 4QL, UK
¹² Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, 14482 Potsdam, Germany
¹³ INAF – Osservatorio Astronomico di Cagliari, Via della Scienza 5, 09047 Selargius (CA), Italy
¹⁴ The American University of Paris, 2bis, Passage Landrieu 75007 Paris, France

Received: 13 October 2021
Accepted: 4 March 2022

Abstract

We present one of the very first extensive classifications of a large sample of molecular clouds based on their morphology. This is achieved using a recently published catalogue of 10 663 clouds obtained from the first data release of the Structure, Excitation and Dynamics of the Inner Galactic InterStellar Medium (SEDIGISM) survey. The clouds are classified into four different morphologies via visual inspection and using an automated algorithm – J plots. The visual inspection also serves as a test for the J plots algorithm as this is the first time it has been used on molecular gas. Generally, it has been found that the structure of molecular clouds is highly filamentary, and our observations indeed verify that most of our molecular clouds are elongated structures. Based on our visual classification of the 10 663 SEDIGISM clouds, 15% are ring-like, 57% are elongated, 15% are concentrated, and 10% are clumpy clouds. The remaining clouds do not belong to any of these morphology classes and are termed unclassified. We compare the SEDIGISM molecular clouds with structures identified through other surveys: the elongated structures from the APEX Telescope Large Area Survey of the Galaxy (ATLASGAL) and the bubbles from Milky Way Project (MWP). We find that many of the ATLASGAL and MWP structures are velocity coherent. Elongated ATLASGAL structures overlap with ≈21% of the elongated SEDIGISM structures (elongated and clumpy clouds), and MWP bubbles overlap with ≈25% of the ring-like SEDIGISM clouds. We also analyse the star formation associated with different cloud morphologies using two different techniques. The first technique examines star formation efficiency and the dense gas fraction based on SEDIGISM cloud and ATLASGAL clump data. The second technique uses the highmass star formation threshold for molecular clouds. The results indicate that clouds with ring-like and clumpy morphologies show a higher degree of star formation.