Properties and rotation of molecular clouds in M 33

  title={Properties and rotation of molecular clouds in M 33},
  author={J. Braine and Erik W. Rosolowsky and Pierre Gratier and Edvige Corbelli and Karl F. Schuster},
  journal={arXiv: Astrophysics of Galaxies},
The sample of 566 molecular clouds identified in the CO(2--1) IRAM survey covering the disk of M~33 is explored in detail.The clouds were found using CPROPS and were subsequently catalogued in terms of their star-forming properties as non-star-forming (A), with embedded star formation (B), or with exposed star formation C.We find that the size-linewidth relation among the M~33 clouds is quite weak but, when comparing with clouds in other nearby galaxies, the linewidth scales with average… 

Rotation of molecular clouds in M 51

The grand-design spiral galaxy M 51 was observed at 40 pc resolution in CO(1–0) by the PAWS project. A large number of molecular clouds were identified and we search for velocity gradients in two

Rise and fall of molecular clouds across the M 33 disk

We carried out deep searches for CO line emission in the outer disk of M 33, at R >  7 kpc, and examined the dynamical conditions that can explain variations in the mass distribution of the molecular

Rotation of Two Micron All Sky Survey Clumps in Molecular Clouds

We have analyzed the rotational properties of 12 clumps using 13CO (1–0) and C18O (1–0) maps of the Five College Radio Astronomy Observatory 13.7 m radio telescope. The clumps, located within

Probability distribution functions of gas surface density in M 33

Aims. We examine the interstellar medium (ISM) of M 33 to unveil fingerprints of self-gravitating gas clouds throughout the star-forming disk. Methods. The probability distribution functions (PDFs)

ALMA resolves giant molecular clouds in a tidal dwarf galaxy

Tidal dwarf galaxies (TDGs) are gravitationally bound condensations of gas and stars that formed during galaxy interactions. Here we present multi-configuration ALMA observations of J1023+1952, a TDG

Northern Galactic molecular cloud clumps in Hi-GAL: dense gas map and environmental trends

In the quest to understand high-mass star formation, it is necessary to understand that from which the high-mass stars will form -- the dense molecular gas clouds and clumps. The Herschel infrared

Comparing the properties of GMCs in M33 from simulations and observations

We compare the properties of clouds in simulated M33 galaxies to those observed in the real M33. We apply a friends of friends algorithm and CPROPS to identify clouds, as well as a pixel by pixel

The changing GMC population in galaxy interactions

With the advent of modern observational efforts providing extensive giant molecular cloud catalogues, understanding the evolution of such clouds in a galactic context is of prime importance. While

Fragmentation of star-forming filaments in the X-shaped nebula of the California molecular cloud

Dense molecular filaments are central to the star formation process, but the detailed manner in which they fragment into prestellar cores is not yet well understood. Here, we investigate the

Giant molecular cloud catalogues for PHANGS-ALMA: methods and initial results

We present improved methods for segmenting CO emission from galaxies into individual molecular clouds, providing an update to the cprops algorithms presented by Rosolowsky & Leroy. The new code



Giant Molecular Clouds in M33. II. High-Resolution Observations

We present 12CO (J = 1 → 0) observations of 45 giant molecular clouds (GMCs) in M33 made with the BIMA array. The observations have a linear resolution of 20 pc, sufficient to measure the sizes of

Giant molecular clouds in the Local Group galaxy M 33

We present an analysis of the systematic CO(2-1) survey at 12" resolution covering most of the local group spiral M 33 which, at a distance of 840 kpc, is close enough that individual giant molecular

The properties of individual giant molecular clouds in M33

A total of 19 fields in the nearby spiral galaxy M33 have been observed by millimeter-wave interferometer at about 30 pc resolution. A total of 38 individual giant molecular clouds (GMCs) were

Giant Molecular Clouds in M33. I. BIMA All-Disk Survey

We present the first interferometric 12CO (J = 1 → 0) map of the entire Hα disk of M33. The 13″ diameter synthesized beam corresponds to a linear resolution of 50 pc, sufficient to distinguish

Molecular cloud formation and the star formation efficiency in M 33 - Molecule and star formation in M 33

Does star formation proceed in the same way in large spirals such as the Milky Way and in smaller chemically younger galaxies? Earlier work suggests a more rapid transformation of H2 into stars in

The Mass Spectra of Giant Molecular Clouds in the Local Group

We reanalyze the catalogs of molecular clouds in the Local Group to determine the parameters of their mass distributions in a uniform manner. The analysis uses the error‐in‐variables method of

Physical properties of giant molecular clouds in the Large Magellanic Cloud

The Magellanic Mopra Assessment (MAGMA) is a high angular resolution ^(12)CO (J = 1 → 0) mapping survey of giant molecular clouds (GMCs) in the Large Magellanic Cloud (LMC) and Small Magellanic Cloud

From molecules to young stellar clusters: the star formation cycle across the disk of M 33

Aims. We study the association between giant molecular clouds (GMCs) and young stellar cluster candidates (YSCCs) to shed light on the time evolution of local star formation episodes in the nearby

Angular Momentum in Giant Molecular Clouds. II. M33

We present an analysis comparing the properties of 45 giant molecular clouds (GMCs) in M33 and the atomic hydrogen (H i) with which they are associated. High-resolution Very Large Array observations

The varying mass distribution of molecular clouds across M83

The work of Adamo et al. showed that the mass distributions of young massive stellar clusters were truncated above a maximum-mass scale in the nearby galaxy M83 and that this truncation mass varies