The Initial Mass Function of the Stellar Association NGC 602 in the Small Magellanic Cloud with<i>Hubble Space Telescope</i>ACS Observations

Schmalzl, M.; Gouliermis, D. A.; Dolphin, Andrew E.; Henning, Thomas

doi:10.1086/588722

Cited by 39 publications

(61 citation statements)

References 49 publications

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“…Nonetheless, it is likely that the production history of nitrogen is not the same between the SMC and the MB. The IMF of a stellar association NGC 602 in the SMC (a single power law with a slope of Γ ∼ −1.2 for M/M = 1-45; Schmalzl et al 2008) is quite similar to the IMF in the solar neighborhood (Γ ∼ −1.35 for M/M = 0. 4-10;Salpeter 1955).…”

Section: Comparison With Dla Systems At High-zmentioning

confidence: 81%

The Magellanic Bridge as a Damped Lyman Alpha System: Physical Properties of Cold Gas Toward PKS 0312-770

Misawa

Charlton

Kobulnicky

et al. 2009

ApJ

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We measure the physical properties of a local multicomponent absorption-line system at V ∼200 km s −1 toward the quasar PKS 0312-770 behind the Magellanic Bridge (MB) using Hubble Space Telescope Space Telescope Imaging Spectrograph (STIS) spectroscopy in conjunction with photoionization modeling. At an impact parameter of ∼10 kpc from the Small Magellanic Cloud (SMC), this sightline provides a unique opportunity to probe the chemical properties and ionization structure in a nearby absorption line system with a column density of log N H i ∼20.2, at the transition between damped Lyα (DLA) and sub-DLA systems. We find that metallicity of −1.0 < log(Z/Z ) < −0.5 and ionization parameter of −6 < log U < −5 for three low-ionization components and log U ∼ −2.6 for one high-ionization component. One component at V = 207 km s −1 shows an α-element abundance log(Si/H) ∼ −5.0, making it ∼0.2 dex more metal-rich than both SMC H ii regions and stars within the MB and the SMC. The N/Si ratio in this component is log(N/Si) = −0.3 ± 0.1, making it comparable to other N-poor dwarf galaxies and ∼0.2 dex lower than H ii regions in the SMC. Another component at V = 236 km s −1 shows a similar Si/H ratio but has log(N/Si) = −1.0 ± 0.2, indicating a nitrogen deficiency comparable to that seen in the most N-poor DLA systems. These differences imply different chemical enrichment histories between components along the same sightline. Our results suggest that if these absorbers are representative some fraction of DLA systems, then (1) DLA systems along single sightlines do not necessarily represent the global properties of the absorbing cloud, and (2) the chemical composition within a given DLA cloud may be inhomogeneous.

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Section: Comparison With Dla Systems At High-zmentioning

confidence: 81%

The Magellanic Bridge as a Damped Lyman Alpha System: Physical Properties of Cold Gas Toward PKS 0312-770

Misawa

Charlton

Kobulnicky

et al. 2009

ApJ

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“…Although this IMF seems to flatten for masses close to solar, no important change in the slope is identified. We found that, in general, a single-power law with a slope of α −2.2 ± 0.3 represents well the average IMF of the system as it is constructed with the use of all considered grids of models (Schmalzl et al 2008). This result is in line with that of Sabbi et al (2008) for NGC 346.…”

Section: Low-mass Pms Populations In the Magellanic Cloudsmentioning

confidence: 67%

“…Our photometric study of another young SMC star cluster, NGC 602, with HST/ACS revealed a coherent sample of PMS stars, ideal for the study of the low-mass IMF in the SMC and the complications in its construction (Schmalzl et al 2008). The IMF of the PMS population of NGC 602 was constructed by counting the stars between evolutionary tracks on the CMD (Fig.…”

Section: Low-mass Pms Populations In the Magellanic Cloudsmentioning

confidence: 99%

The sub-solar initial mass function in the Large Magellanic Cloud

Gouliermis

2008

Proc. IAU

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Abstract. The Magellanic Clouds offer a unique variety of star forming regions seen as bright nebulae of ionized gas, related to bright young stellar associations. Nowadays, observations with the high resolving efficiency of the Hubble Space Telescope allow the detection of the faintest infant stars, and a more complete picture of clustered star formation in our dwarf neighbors has emerged. I present results from our studies of the Magellanic Clouds, with emphasis in the young low-mass pre-main sequence populations. Our data include imaging with the Advanced Camera for Surveys of the association LH 95 in the Large Magellanic Cloud, the deepest observations ever taken with HST of this galaxy. I discuss our findings in terms of the initial mass function, which we constructed with an unprecedented completeness down to the sub-solar regime, as the outcome of star formation in the low-metallicity environment of the LMC.

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“…The slopes are also close to the Salpeter value, supporting the idea of a universal IMF. Schmalzi et al (2008) hand, at lower masses (m/m ⊙ < 1), the existence of a universal IMF is still in debate (see contribution by D. Gouliermis in these proceedings). A clear evidence of structural evolution of star clusters is given by the relation between core size (R c ) and age.…”

Section: Magellanic Star Clusters In High Resolution: Structure and Dmentioning

confidence: 99%

The star clusters of the Magellanic System

Santiago

2008

Proc. IAU

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Abstract. More than 50 years have elapsed since the first studies of star clusters in the Magellanic Clouds. The wealth of data accumulated since then has not only revealed a large cluster system, but also a diversified one, filling loci in the age, mass and chemical abundance parameter space which are complementary to Galactic clusters. Catalogs and photometric samples currently available cover most of the cluster mass range. The expectations of relatively long cluster disruption timescales in the Clouds have been confirmed, allowing reliable assessments of the cluster initial mass function and of the cluster formation rate in the Clouds. Due to their proximity to the Galaxy, Magellanic clusters are also well resolved into stars. Analysis of colour-magnitude diagrams (CMDs) of clusters with different ages, masses and metallicities are useful tools to test dynamical effects such as mass loss due to stellar evolution, two-body relaxation, stellar evaporation, cluster interactions and tidal effects. The existence of massive and young Magellanic clusters has provided insight into the physics of cluster formation. The magnitudes and colours of different stellar types are confronted with stellar evolutionary tracks, thus constraining processes such as convective overshooting, stellar mass-loss, rotation and pre main-sequence evolution. Finally, the Magellanic cluster system may contribute with nearby and well studied counterparts of recently proposed types of extragalactic clusters, such as Faint Fuzzies and Diffuse Star Clusters.

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The Initial Mass Function of the Stellar Association NGC 602 in the Small Magellanic Cloud withHubble Space TelescopeACS Observations

Cited by 39 publications

References 49 publications

The Magellanic Bridge as a Damped Lyman Alpha System: Physical Properties of Cold Gas Toward PKS 0312-770

The Magellanic Bridge as a Damped Lyman Alpha System: Physical Properties of Cold Gas Toward PKS 0312-770

The sub-solar initial mass function in the Large Magellanic Cloud

The star clusters of the Magellanic System

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