First Results of a CO Survey of the Small Magellanic Cloud with NANTEN

Mizuno, N.; Rubio, M.; Mizuno, Akira; Yamaguchi, Ryuichi; Onishi, Toshikazu; Fukui, Y.

doi:10.1093/pasj/53.6.l45

Cited by 111 publications

(169 citation statements)

References 18 publications

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“…Mizuno et al (2001a) find that young emission objects are positionally well correlated with CO clouds, while emissionless objects of ages ∼6−100 Myr do not show any correlation to the CO clouds. Emission objects were excluded from our sample, so we cannot investigate their possible association with CO clouds.…”

Section: Spatial Age Distribution Smcmentioning

confidence: 73%

Ages and luminosities of young SMC/LMC star clusters and the recent star formation history of the Clouds

Glatt

Grebel

Koch

2010

A&A

170

213

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Aims. In this paper we discuss the age and spatial distribution of young (age < 1 Gyr) Small Magellanic Cloud (SMC) and Large Magellanic Cloud (LMC) clusters using data from the Magellanic Cloud Photometric Surveys. Luminosities are calculated for all age-dated clusters. Methods. The ages of 324 and 1193 populous star clusters in the SMC and the LMC were determined fitting Padova and Geneva isochrone models to their resolved color-magnitude diagrams. The clusters cover an age range between 10 Myr and 1 Gyr in each galaxy. For the SMC, a constant distance modulus of (m − M) 0 = 18.90 and a metallicity of Z = 0.004 were adopted. For the LMC, we used a constant distance modulus of (m − M) 0 = 18.50 and a metallicity of Z = 0.008. For both galaxies, we used a variable color excess to derive the cluster ages. Results. We find two periods of enhanced cluster formation in both galaxies at 160 Myr and 630 Myr (SMC) and at 125 Myr and 800 Myr (LMC). We present the spatially resolved recent star formation history of both Clouds based on young star clusters. The first peak may have been triggered by a close encounter between the SMC and the LMC. In both galaxies, the youngest clusters reside in the supergiant shells, giant shells, the intershell regions, and toward regions with a high Hα content, suggesting that their formation is related to expansion and shell-shell interaction. Most of the clusters are older than the dynamical age of the supergiant shells. No evidence of cluster dissolution was found. Computed V band luminosities show a trend toward fainter magnitudes with increasing age, as well as a trend toward brighter magnitudes with increasing apparent cluster radii.

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Section: Spatial Age Distribution Smcmentioning

confidence: 73%

Ages and luminosities of young SMC/LMC star clusters and the recent star formation history of the Clouds

Glatt

Grebel

Koch

2010

A&A

170

213

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“…Under this assumption, based on early CO(1−0) observations with the CTIO/Columbia mm telescope and the SEST, Rubio et al (1993) found X SMC to be size dependent and equal to 3.9 × (R/10 pc) −0.7 X Gal where R is the cloud radius, defined as √ (A/π). The SMC NANTEN survey (Mizuno et al 2001), with a linear resolution of 40 pc, found consistently an average conversion factor X SMC ∼ 9X Gal . The CO(1−0) luminosity of SMCB1-1 is 1.2 × 10 3 K km s −1 (Rubio et al 1996) which multiplied by the appropriate X factor gives M(H 2 ) co = 2.7 × 10 4 M in Table 1.…”

Section: Gas Massmentioning

confidence: 88%

Millimeter dust emission from an SMC cold molecular cloud

Rubio¹,

Boulanger

Rantakyrö

et al. 2004

A&A

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Abstract. We presented SIMBA 1.2 mm continuum observations of SMCB1-1 an SMC molecular cloud known to be distant from massive ionizing stars. The gas mass derived from the SIMBA flux is a factor of ∼10 higher than the virial mass previously reported from CO observations. We propose an interpretation where the virial mass underestimates the total mass because the CO emission comes from dense clumps which do not trace the full cloud area and velocity distribution. This work sets an important question for the understanding of star formation in low metallicity gas. Do CO observations grossly underestimate the amount of dense self gravitating clouds where stars can form?

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“…Recent studies of Local Group galaxies have surveyed large numbers of molecular clouds in the Large Magellanic Cloud (Mizuno et al 2001b), the Small Magellanic Cloud (Mizuno et al 2001a), M33 , and a bevy of Local Group dwarf galaxies (e.g., Wilson 1994;Taylor et al 1999). These recent studies explore the nature of star formation on galactic scales by studying the properties of giant molecular clouds (GMCs, M > 10 5 M ) throughout their host galaxies.…”

Section: Introductionmentioning

confidence: 99%

Giant Molecular Clouds in M31. I. Molecular Cloud Properties

Rosolowsky

2007

ApJ

113

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We present Berkeley-Illinois-Maryland Association ( BIMA) millimeter interferometer observations of giant molecular clouds (GMCs) along a spiral arm in M31. The observations consist of a survey using the compact configuration of the interferometer and follow-up, higher resolution observations on a subset of the detections in the survey. The data are processed using an analysis algorithm designed to extract GMCs and correct their derived properties for observational biases, thereby facilitating comparison with Milky Way data. The algorithm identifies 67 GMCs, of which 19 have a sufficient signal-to-noise ratio to accurately measure their properties. The GMCs in this portion of M31 are indistinguishable from those found in the Milky Way, having a similar size-line width relationship and distribution of virial parameters, confirming the results of previous, smaller studies. The velocity gradients and angular momenta of the GMCs are comparable to the values measured in M33 and the Milky Way, and in all cases are below expected values based on the local galactic shear. The studied region of M31 has an interstellar radiation field, metallicity, Toomre Q parameter, and midplane volume density similar to those of the inner Milky Way, so the similarity of GMC populations between the two systems is not surprising.

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First Results of a CO Survey of the Small Magellanic Cloud with NANTEN

Cited by 111 publications

References 18 publications

Ages and luminosities of young SMC/LMC star clusters and the recent star formation history of the Clouds

Ages and luminosities of young SMC/LMC star clusters and the recent star formation history of the Clouds

Millimeter dust emission from an SMC cold molecular cloud

Giant Molecular Clouds in M31. I. Molecular Cloud Properties

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