On the structure of molecular clouds [PDF]
Monthly Notices of the Royal Astronomical Society, 2012 We show that the inter-cloud Larson scaling relation between mean volume density and size $ \propto R^{-1}$, which in turn implies that mass $M\propto R^2$, or that the column density $N$ is constant, is an artifact of the observational methods used.
Ballesteros-Paredes +5 more
openaire +5 more sources
Molecular line signatures of cloud–cloud collisions [PDF]
Monthly Notices of the Royal Astronomical Society, 2021 ABSTRACT Collisions between interstellar gas clouds are potentially an important mechanism for triggering star formation. This is because they are able to rapidly generate large masses of dense gas. Observationally, cloud collisions are often identified in position–velocity (PV) space through bridging features between intensity peaks ...
Anthony Peter Whitworth, F. D. Priestley
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The anatomy of the Orion B Giant Molecular Cloud: A local template for studies of nearby galaxies [PDF]
, 2016 We aim to develop the Orion B Giant Molecular Cloud (GMC) as a local template for interpreting extra-galactic molecular line observations. We use the wide-band receiver at the IRAM-30m to spatially and spectrally resolve the Orion B GMC. The observations
J. Pety +13 more
semanticscholar +1 more source
Primordial molecular clouds [PDF]
Conference on 3K cosmology, 1999 12 pages, 1 figures, Invited Talk at 3K Cosmology Conference-Roma October ...
D. Puy, M. Signore
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Star cluster formation in a turbulent molecular cloud self-regulated by photoionization feedback [PDF]
, 2017 Most stars in the Galaxy are believed to be formed within star clusters from collapsing molecular clouds. However, the complete process of star formation, from the parent cloud to a gas-free star cluster, is still poorly understood.
E. Gavagnin +3 more
semanticscholar +1 more source
The Galactic Center Molecular Cloud Survey. I. A Steep Linewidth-Size Relation & Suppression of Star Formation [PDF]
, 2016 The Central Molecular Zone (CMZ; inner $\sim{}200~\rm{}pc$) of the Milky Way is a star formation (SF) environment with very extreme physical properties.
J. Kauffmann +14 more
semanticscholar +1 more source
Molecular Cloud Evolution VI. Measuring cloud ages [PDF]
, 2018 This article has been published in Monthly Notices of the Royal Astronomical Society © 2018 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society.
Ansdell +84 more
core +2 more sources
The Survey of Water and Ammonia in the Galactic Center (SWAG): Molecular Cloud Evolution in the Central Molecular Zone [PDF]
, 2017 The Survey of Water and Ammonia in the Galactic Center (SWAG) covers the Central Molecular Zone (CMZ) of the Milky Way at frequencies between 21.2 and 25.4 GHz obtained at the Australia Telescope Compact Array at ∼0.9 pc spatial and ∼2.0 km s−1 spectral ...
N. Krieger +23 more
semanticscholar +1 more source
Filaments in the Lupus molecular clouds [PDF]
Monthly Notices of the Royal Astronomical Society, 2015 We have studied the filaments extracted from the column density maps of the nearby Lupus 1, 3, and 4 molecular clouds, derived from photometric maps observed with the Herschel satellite. Filaments in the Lupus clouds have quite low column densities, with a median value of $\sim$1.5$\times$10$^{21}$ cm$^{-2}$ and most have masses per unit length lower ...
Davide Elia +23 more
openaire +9 more sources
The Large-scale J=3-2 and J=2-1 CO Emission from M17 and its Implications for Extragalactic CO Observations [PDF]
, 1999 We observed a 10x20 pc region of the molecular cloud M17 in the 12CO and 13CO J=3-2 and J=2-1 transitions to determine their global behavior and to assess the reliability of using ratios of CO line intensities integrated over an entire cloud to determine
Aalto S. +17 more
core +3 more sources