An H I Mosaic of the Small Magellanic Cloud

Sault, R. J.; McConnell, D.; Kesteven, M. J.; Hatzidimitriou, D.; Freeman, K. C.; Dopita, M. A.

doi:10.1017/s1323358000019986

Cited by 98 publications

(147 citation statements)

References 9 publications

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“…We confirm the findings of C06 about the discontinuity in the spatial distribution of younger clusters in the supershells 37 A and 304 A. That is, the youngest objects are found toward the eastern rim of the shell (37A) where gas and dust are located (Staveley-Smith et al 1997;Stanimirovic et al 1999) and toward regions luminous in Hα. Such HII regions visible in Hα indicate the presence of massive stars (e.g., OB-stars, supergiants, luminous blue variable stars), supernova remnants, or diffuse ionized nebulae.…”

Section: Spatial Age Distribution Smcsupporting

confidence: 90%

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

Glatt

Grebel

Koch

2010

A&A

166

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 Smcsupporting

confidence: 90%

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

Glatt

Grebel

Koch

2010

A&A

166

213

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“…Its isolation from other regions of massive star formation and the relatively simple surrounding Hi shell structure encouraged us to try to constrain the processes that may have led to its formation. Using the shell catalog derived from the 21 cm neutral hydrogen (Hi) spectrum survey data (Staveley-Smith et al 1997;Staminirovíc et al 1999) we identified a distinct Hi cloud component that is likely the progenitor cloud of the cluster and the Hii region which probably formed in blister fashion from the cloud's periphery. A comparison between Hi and Hii kinematics suggests that star formation in NGC 602 was triggered by compression and turbulence associated with Hi shell interaction ∼ 7 Myr ago (Nigra et al 2008).…”

Section: Ngc 602 Kinematicsmentioning

confidence: 99%

Young Star Clusters in the Small Magellanic Cloud: Impact of Local and Global Conditions on Star Formation

et al. 2008

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Abstract. We compared deep images acquired with the Advanced Camera for Surveys on board of the Hubble Space Telescope with mid-IR Spitzer Space Telescope images and University College London Echelle Spectrograph spectra of NGC 346 and NGC 602, two of the youngest star clusters in the Small Magellanic Cloud. Our multi-wavelength approach allowed us to infer very different origins for the clusters: while NGC 346 is likely the result of the hierarchical collapse of a giant molecular cloud, NGC 602 is probably the result of the collision and consequent interaction of two H I shells of gas.

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“…concentrated towards this part of N66 (Staveley-Smith et al 1997;Stanimirović et al 1999;Gouliermis et al 2008). The H i…”

Section: Morphologymentioning

confidence: 93%

A very young component in the pre-eminent starburst region of the Small Magellanic Cloud

Heydari-Malayeri

Selier

2010

A&A

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Context. Despite extensive research on various components of the N66/NGC 346 complex, few studies have so far focused on N66A, which is a special object in the whole complex and therefore deserves scrutiny. The study of this compact H ii region and its fellow objects seems important in the framework of massive star formation in the Magellanic Clouds.Aims. We present a study of the compact H ii region N66A in the SMC pre-eminent starburst region N66/NGC 346.Methods. This analysis is based mainly on our optical ESO NTT observations, both imaging and spectroscopy, coupled with archive HST ACS data and Spitzer infrared images (IRAC 3.6, 4.5, 5.8, and 8.0 μm).Results. We derive a number of physical characteristics of the compact H ii region N66A. For the first time using spectroscopy, we present the spectral classification of the main exciting star of N66A. Its spectral features indicate that it is a main-sequence massive star of type O8. We compare this result with that based on the stellar Lyman continuum flux estimated from the ionized gas Hβ flux.The compact H ii region belongs to a rare class of H ii regions in the Magellanic Clouds, called high-excitation blobs (HEBs). We propose that N66A probably represents a very young massive star formation event in the N66 complex that has a range of ages.

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An H I Mosaic of the Small Magellanic Cloud

Cited by 98 publications

References 9 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

Young Star Clusters in the Small Magellanic Cloud: Impact of Local and Global Conditions on Star Formation

A very young component in the pre-eminent starburst region of the Small Magellanic Cloud

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