The Second Survey of the Molecular Clouds in the Large Magellanic Cloud by NANTEN. I. Catalog of Molecular Clouds

By Y. Fukui, A. Kawamura, T. Minamidani, Y. Mizuno, Y. Kanai, N. Mizuno, T. Onishi, Y. Yonekura, A. Mizuno, H. Ogawa and 4 more. 2008

225 citations recorded by the source corpus.

The second survey of the molecular clouds in the Large Magellanic Cloud in 12CO (J = 1–0) was carried out by NANTEN. The sensitivity of this survey is twice as high as that of the previous NANTEN survey, leading to a detection of molecular clouds with MCO ≳ 2 × 104 M☉. We identified 272 molecular clouds, 230 of which are detected at three or more observed positions. We derived the physical properties, such as size, line width, and virial mass, of the 164 GMCs that have an extent more than the beam size of NANTEN in both the major and minor axes. The CO luminosity and virial mass of the clouds show a good correlation of Mvir ∝ LCO1.1 ± 0.1, with a Spearman rank correlation of 0.8, suggesting that the clouds are in nearly virial equilibrium. Assuming the clouds are in virial equilibrium, we derived an XCO-factor of ~7 × 1020 cm−2 (K km s−1)−1. The mass spectrum of the clouds is fitted well by a power law of Ncloud(> MCO) ∝ MCO−0.75 ± 0.06 above the completeness limit of 5 × 104 M☉. The slope of the mass spectrum becomes steeper if we fit only the massive clouds, e.g., Ncloud(> MCO) ∝ MCO−1.2 ± 0.2 for MCO ⩾ 3 × 105 M☉.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/4168b98f6a2d5a2903131ca2d1bc84a3b4b81b83

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Instrumentation

Citations in the corpus

THE SECOND SURVEY OF THE MOLECULAR CLOUDS IN THE LARGE MAGELLANIC CLOUD BY NANTEN. II. STAR FORMATION (2009, methodology): “′6 and covered ∼30 deg2 (Fukui et al. 2008).”
The CO-to-H2 Conversion Factor (2013, methodology): “For example, Hughes et al. (2010) find XCO,20 ≈ 4 in the LMC (as do Israel et al. 2003; Pineda et al. 2009; Wong et al. 2011) compared to XCO,20 ≈ 7 found by Fukui et al. (2008) using similar methodology but with ∼ 3 times coarser linear resolution.”
STELLAR FEEDBACK IN MOLECULAR CLOUDS AND ITS INFLUENCE ON THE MASS FUNCTION OF YOUNG STAR CLUSTERS (2009, background): “(3b) We now evaluate Equations (3a) and (3b) with βo = −1.7, the observed exponent of the mass function of molecular clouds (Rosolowsky 2005; Reid &Wilson 2006; Muñoz et al. 2007; Wong et al. 2008; Fukui et al. 2008).”
Planck 2015 results - XXVIII. The Planck Catalogue of Galactic cold clumps (2015, unknown): “After re-scaling for the lower dust-to-gas ratio in the LMC and accounting for mismatches between the intrinsic source size and the Planck and Mopra beam widths, the catalogued masses of the LMC PGCC sources are in good agreement with the masses derived from the Mopra CO data.”
The structure of the interstellar medium of star‐forming galaxies (2011, result): “These surface densities (and corresponding size–mass relation) and their scatter are quite similar to those observed in MW- and SMC-like local galaxies (Bolatto et al. 2008; Fukui et al. 2008; Wong et al. 2008; Goodman, Pineda & Schnee 2009).”
THE PdBI ARCSECOND WHIRLPOOL SURVEY (PAWS): ENVIRONMENTAL DEPENDENCE OF GIANT MOLECULAR CLOUD PROPERTIES IN M51 (2014, background): “This kind of approach can be sufficient to catalog discrete molecular structures in irregular and flocculent galaxies, where the emission is typically sparsely distributed within the observed field (e.g., the LMC, Wong et al. 2011).”
The SILCC (SImulating the LifeCycle of molecular Clouds) project - II. Dynamical evolution of the supernova-driven ISM and the launching of outflows (2015, result): “To a similar level, our molecular dispersions agree with other GMC measurements in M31 (Rosolowsky 2007), the LMC (Fukui et al. 2008), and the SMC (Mizuno et al. 2001, see also the review by Fukui & Kawamura 2010).”
Non-standard grain properties, dark gas reservoir, and extended submillimeter excess, probed by Herschel in the Large Magellanic Cloud (2011, background): “We assume a constant CO-to-H2 conversion factor of XCO = 7 × 1020 H cm−2(K km s−1)−1, based on the virial estimate of Fukui et al. (2008).”
NEW OPTICAL REDDENING MAPS OF THE LARGE AND SMALL MAGELLANIC CLOUDS (2011, methodology): “In Figure 22 the map of molecular hydrogen clouds as observed by NANTEN (Fukui et al. 2008), and traced by CO, is superimposed with the reddening from the RR Lyrae stars.”
STAR FORMATION IN DISK GALAXIES. I. FORMATION AND EVOLUTION OF GIANT MOLECULAR CLOUDS VIA GRAVITATIONAL INSTABILITY AND CLOUD COLLISIONS (2008, background): “Fukui et al. (2008) studied 164 GMCs in the Large Magellanic Cloud, concluding these clouds were also close to virial equilibrium.”
THE MAGELLANIC MOPRA ASSESSMENT (MAGMA). I. THE MOLECULAR CLOUD POPULATION OF THE LARGE MAGELLANIC CLOUD (2011, background): “The survey targets include the most luminous GMCs detected in the second NANTEN survey (Fukui et al. 2008).”
Molecular and atomic gas in the Local Group galaxy M 33 (2010, result): “Earlier studies of GMCs in M33 include Wilson et al. (1997) and Rosolowsky et al. (2003) and studies similar to our own of other Local Group galaxies have been made by e.g. Fukui et al. (2008); Israel et al. (2003); Leroy et al. (2006); Nieten et al. (2006).”
FIRE-2 simulations: physics versus numerics in galaxy formation (2017, background): “…dispersion of gas within clouds, versus their projected mass-weighted rms radius), to observations of nearby galaxies ((Bolatto et al. 2008; Fukui et al. 2008; Heyer et al. 2009; Muraoka et al. 2009; Roman-Duval et al. 2010; Colombo et al. 2014; Heyer & Dame 2015; Tosaki et al. 2017); note…”
LOW CO LUMINOSITIES IN DWARF GALAXIES (2012, background): “…MB, SFR, and metallicity, but we are able to detect them at distances D = 2.9−9.5 Mpc. Galaxies that have not been detected when stacking over the entire galaxy extent, have LCO 2−1 upper limits 0.1 − 2.6 times the CO luminosity of the LMC, LLMCCO 1−0 = 3.2 × 106 K km s−1 pc2 (Fukui et al. 2008).”
MOLECULAR GAS AND STAR FORMATION IN NEARBY DISK GALAXIES (2013, background): “Low surface density GMCs or significant contribution of “translucent” (AV ∼ 1–2 mag) gas to the overall CO emission are supported by observations of the Milky Way Heyer et al. (2009) and Liszt et al. (2010), LMC observations by Hughes et al. (2010); Wong et al. (2011), and M31 (Schruba et al. in pre”