ERRATUM: “THE MAGELLANIC MOPRA ASSESSMENT (MAGMA). I. THE MOLECULAR CLOUD POPULATION OF THE LARGE MAGELLANIC CLOUD” (2011, ApJS, 197, 16)

Wong, Tony; Hughes, Annie; Ott, J.; Müller, Erik; Pineda, J. L.; Bernard, J. P.; Chu, Y. H.; Fukui, Y.; Gruendl, R. A.; Henkel, C.; Kawamura, Akiko; Klein, U.; Looney, Leslie W.; Maddison, Sarah; Mizuno, Yumiko; Paradis, D.; Seale, Jonathan; Welty, D. E.

doi:10.1088/0067-0049/208/1/13

Cited by 114 publications

(254 citation statements)

References 2 publications

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“…Earlier studies have found a large range for the power law index of GMC mass functions in nearby galaxies, from β PL = −1.5 in the inner disk of the Milky Way (Rice et al 2016) to β PL = −2.6 in the LMC (Wong et al 2011) and β PL = −2.9 in M33 (Rosolowsky 2005). There are also some discrepancies among the published indices, such as β PL = −1.7 for the LMC (Blitz et al 2007) and β PL = −2.3 for M33 (Gratier et al 2012).…”

Section: The Shape Of the Gmc Mass Functionsmentioning

confidence: 97%

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Mass Functions of Giant Molecular Clouds and Young Star Clusters in Six Nearby Galaxies

Mok

Chandar

Fall

2020

ApJ

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We compare the mass functions of young star clusters (ages ≤ 10 Myr) and giant molecular clouds (GMCs) in six galaxies that cover a large range in mass, metallicity, and star formation rate (LMC, M83, M51, NGC 3627, the Antennae, and NGC 3256). We perform maximum-likelihood fits of the Schechter function, ψ(M ) = dN/dM ∝ M β exp(−M/M * ), to both populations. We find that most of the GMC and cluster mass functions in our sample are consistent with a pure power-law distribution (M * → ∞). M51 is the only galaxy that shows some evidence for an upper cutoff (M * ) in both populations. Therefore, physical upper mass cutoffs in populations of both GMCs and clusters may be the exception rather than the rule. When we perform power-law fits, we find a range of indices β PL = −2.3 ± 0.3 for our GMC sample and β PL = −2.0 ± 0.3 for the cluster sample. This result, that β Clusters ≈ β GMC ≈ −2, is consistent with theoretical predictions for cluster formation and suggests that the star-formation efficiency is largely independent of mass in the GMCs.

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Section: The Shape Of the Gmc Mass Functionsmentioning

confidence: 97%

“…• LMC: A catalog of 543 GMCs was published by Wong et al (2011), based on CO(1-0) observations taken with the ATNF Mopra Telescope. They assume a value for the CO-to-H 2 (α CO ) conversion factor of 4.8 M (K km s −1 pc 2 ) −1 .…”

Section: Previous Catalogsmentioning

confidence: 99%

Mass Functions of Giant Molecular Clouds and Young Star Clusters in Six Nearby Galaxies

Mok

Chandar

Fall

2020

ApJ

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“…The molecular gas properties of these regions are quite different, however. The integrated 12 CO(1−0) luminosity that is observed to be spatially projected onto N157A is ∼ 2.5 × 10 5 K km s −1 pc 2 , corresponding to only ∼ 10 6 M of molecular gas for a Galactic CO-to-H 2 conversion factor (Wong et al 2011;Johansson et al 1998). The young stars in 30 Dor thus appear to have cleared out most of the molecular gas associated with the H ii region, contrary to the headlight cloud, for which we estimate a molecular mass of ≥ 10 7 M .…”

Section: Comparison With 30 Dor In the Lmcmentioning

confidence: 99%

The headlight cloud in NGC 628: An extreme giant molecular cloud in a typical galaxy disk

Herrera

Pety

Hughes

et al. 2020

A&A

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Context. Cloud-scale surveys of molecular gas reveal the link between giant molecular cloud properties and star formation across a range of galactic environments. Cloud populations in galaxy disks are considered to be representative of the 'normal' star formation process, while galaxy centers tend to harbour denser gas that exhibits more extreme star formation. At high resolution, however, molecular clouds with exceptional gas properties and star formation activity may also be observed in normal disk environments. In this paper, we study the brightest cloud traced in CO(2−1) emission in the disk of nearby spiral galaxy NGC 628. Aims. We characterize the properties of the molecular and ionized gas that is spatially coincident with an extremely bright H ii region in the context of the NGC 628 galactic environment. We investigate how feedback and large-scale processes influence the properties of the molecular gas in this region. Methods. High resolution ALMA observations of CO(2−1) and CO(1−0) emission are used to characterize the mass and dynamical state of the "headlight" molecular cloud. The characteristics of this cloud are compared to the typical properties of molecular clouds in NGC 628. A simple large velocity gradient (LVG) analysis incorporating additional ALMA observations of 13 CO(1−0), HCO + (1−0) and HCN(1−0) emission is used to constrain the beam-diluted density and temperature of the molecular gas. We analyze the MUSE spectrum using Starburst99 to characterize the young stellar population associated with the H ii region. Results. The unusually bright headlight cloud is massive (1 − 2 × 10 7 M ), with a beam-diluted density of n H 2 = 5 × 10 4 cm −3 based on LVG modeling. It has a low virial parameter, suggesting that the CO emission associated with this cloud may be overluminous due to heating by the H ii region. A young (2 − 4 Myr) stellar population with mass 3 × 10 5 M is associated. Conclusions. We argue that the headlight cloud is currently being destroyed by feedback from young massive stars. Due to the cloud's large mass, this phase of the cloud's evolution is long enough for the impact of feedback on the excitation of the gas to be observed. The high mass of the headlight cloud may be related to its location at a spiral co-rotation radius, where gas experiences reduced galactic shear compared to other regions of the disk, and receives a sustained inflow of gas that can promote the cloud's mass growth.

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“…Spectral lines are identified with the aid of the Cologne Database for Molecular Spectroscopy 1 (CDMS, Müller et al 2001Müller et al , 2005 and the molecular database of the Jet Propulsion Laboratory 2 (JPL, Pickett et al 1998). The detection criteria adopted here are the 2.5σ significance level and the velocity coincidence with the systemic velocity of nearby CO clouds (between 260 km s −1 and 270 km s −1 , estimated using the MAGMA data presented in Wong et al 2011 Line parameters are measured by fitting a Gaussian profile to observed lines. Based on the fitting, we estimate the peak brightness temperature, the FWHM, the LSR velocity, and the integrated intensity for each line.…”

Section: Data Reductionmentioning

confidence: 99%

Chemistry and Physics of a Low-metallicity Hot Core in the Large Magellanic Cloud

Shimonishi

Das

Sakai

et al. 2020

ApJ

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We here present the results of 0.1 pc-scale observations in 250 and 350 GHz towards a newly-discovered hot molecular core in a nearby low-metallicity galaxy, the Large Magellanic Cloud (LMC), with the Atacama Large Millimeter/submillimeter Array. A variety of C/N/O/Si/S-bearing molecules are detected towards the high-mass young stellar object, ST16. A rotating protostellar envelope is for the first time detected outside our Galaxy by SO 2 and 34 SO lines. An outflow cavity is traced by CCH and CN. The isotope abundance of sulfur in the source is estimated to be 32 S/ 34 S = 17 and 32 S/ 33 S = 53 based on SO, SO 2 , and CS isotopologues, suggesting that both 34 S and 33 S are overabundant in the LMC. Rotation diagram analyses show that the source is associated with hot gas (>100 K) traced by high-excitation lines of CH 3 OH and SO 2 , as well as warm gas (∼50 K) traced by CH 3 OH, SO 2 , 34 SO, OCS, CH 3 CN lines. A comparison of molecular abundances between LMC and Galactic hot cores suggests that organic molecules (e.g., CH 3 OH, a classical hot core tracer) show a large abundance variation in low metallicity, where the present source is classified into an organic-poor hot core. Our astrochemical simulations suggest that different grain temperature during the initial ice-forming stage would contribute to the chemical differentiation. In contrast, SO 2 shows similar abundances within all the known LMC hot cores and the typical abundance roughly scales with the LMC's metallicity. Nitrogen-bearing molecules are generally less abundant in the LMC hot cores, except for NO. The present results suggest that chemical compositions of hot cores do not always simply scale with the metallicity.

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ERRATUM: “THE MAGELLANIC MOPRA ASSESSMENT (MAGMA). I. THE MOLECULAR CLOUD POPULATION OF THE LARGE MAGELLANIC CLOUD” (2011, ApJS, 197, 16)

Cited by 114 publications

References 2 publications

Mass Functions of Giant Molecular Clouds and Young Star Clusters in Six Nearby Galaxies

Mass Functions of Giant Molecular Clouds and Young Star Clusters in Six Nearby Galaxies

The headlight cloud in NGC 628: An extreme giant molecular cloud in a typical galaxy disk

Chemistry and Physics of a Low-metallicity Hot Core in the Large Magellanic Cloud

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