H [CSC]i[/CSC] Shells in the Large Magellanic Cloud

Kim, Sungeun; Dopita, Michael A.; Staveley‐Smith, L.; Bessell, M. S.

doi:10.1086/301116

Cited by 243 publications

(427 citation statements)

References 28 publications

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“…More information on such an investigation can be given from observations on atomic hydrogen (HI) in the LMC, like the ones presented by Kim et al (1999). These authors note that the structure of HI in the LMC is characterised by a large number of shells, as well as of filamentary and spiral structures.…”

Section: Spatial Distribution Of the Systemsmentioning

confidence: 99%

OB stellar associations in the Large Magellanic Cloud: Survey of young stellar systems

Gouliermis

Kontizas

et al. 2003

A&A

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Abstract. The method developed by Gouliermis et al. (2000, Paper I), for the detection and classification of stellar systems in the LMC, was used for the identification of stellar associations and open clusters in the central area of the LMC. This method was applied on the stellar catalog produced from a scanned 1.2 m UK Schmidt Telescope Plate in U with a field of view almost 6.• 5 × 6.• 5, centered on the Bar of this galaxy. The survey of the identified systems is presented here followed by the results of the investigation on their spatial distribution and their structural parameters, as were estimated according to our proposed methodology in Paper I. The detected open clusters and stellar associations show to form large filamentary structures, which are often connected with the loci of HI shells. The derived mean size of the stellar associations in this survey was found to agree with the average size found previously by other authors, for stellar associations in different galaxies. This common size of about 80 pc might represent a universal scale for the star formation process, whereas the parameter correlations of the detected loose systems support the distinction between open clusters and stellar associations.

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Section: Spatial Distribution Of the Systemsmentioning

confidence: 99%

OB stellar associations in the Large Magellanic Cloud: Survey of young stellar systems

Gouliermis

Kontizas

et al. 2003

A&A

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“…The population exhibits correlations with neutral hydrogen structures. The most striking example is the many SNRs (a dozen) around the supergiant shell (SGS) LMC 4 (Meaburn 1980, SGS 11 in the notation of Kim et al 1999). SGSs are formed by the combined action of multiple generations of massive star formation.…”

Section: Comparison With Other Wavelengthsmentioning

confidence: 99%

“…Interpreting the N H fraction is made easier by the favourable orientation of the LMC. Neutral hydrogen is mainly distributed in a nearly circular disc at a moderate inclination angle 22 , with a thickness of ∼360 pc (Kim et al 1999). Small N H fractions ( 0.3, e.g.…”

Section: Adding the Third Dimensionmentioning

confidence: 99%

“…8, star formation is intense around the SGS LMC 4, and the edges of the shell abound in SNRs. Many LMC SGS have not been (fully) surveyed by XMM-Newton, for instance (in the notation of Kim et al 1999) SGS 3 and 6 in the north, SGS 2 and 5 in the west, and SGS 4 in the south. Targeting in particular SGSs associated to star formation (e.g.…”

Section: Summary and Outlooksmentioning

confidence: 99%

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The population of X-ray supernova remnants in the Large Magellanic Cloud

Maggi

Haberl

Kavanagh

et al. 2016

A&A

149

205

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Aims. We present a comprehensive X-ray study of the population of supernova remnants (SNRs) in the Large Magellanic Cloud (LMC). Using primarily XMM-Newton observations, we conduct a systematic spectral analysis of LMC SNRs to gain new insight into their evolution and the interplay with their host galaxy. Methods. We combined all the archival XMM-Newton observations of the LMC with those of our Very Large Programme LMC survey. We produced X-ray images and spectra of 51 SNRs, out of a list of 59 objects compiled from the literature and augmented with newly found objects. Using a careful modelling of the background, we consistently analysed all the X-ray spectra and measure temperatures, luminosities, and chemical compositions. The locations of SNRs are compared to the distributions of stars, cold gas, and warm gas in the LMC, and we investigated the connection between the SNRs and their local environment, characterised by various star formation histories. We tentatively typed all LMC SNRs, in order to constrain the ratio of core-collapse to type Ia SN rates in the LMC. We also compared the column densities derived from X-ray spectra to H i maps, thus probing the three-dimensional structure of the LMC. Results. This work provides the first homogeneous catalogue of the X-ray spectral properties of SNRs in the LMC. It offers a complete census of LMC remnants whose X-ray emission exhibits Fe K lines (13% of the sample), or reveals the contribution from hot supernova ejecta (39%), which both give clues to the progenitor types. The abundances of O, Ne, Mg, Si, and Fe in the hot phase of the LMC interstellar medium are found to be between 0.2 and 0.5 times the solar values with a lower abundance ratio [α/Fe] than in the Milky Way. The current ratio of core-collapse to type Ia SN rates in the LMC is constrained to N CC /N Ia = 1.35( +0.11 −0.24 ), which is lower than in local SN surveys and galaxy clusters. Our comparison of the X-ray luminosity functions of SNRs in Local Group galaxies (LMC, SMC, M31, and M33) reveals an intriguing excess of bright objects in the LMC. Finally, we confirm that 30 Doradus and the LMC Bar are offset from the main disc of the LMC to the far and near sides, respectively.

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“…2. Dust clouds seen in the SPIRE 350 μm image were identified using an automatic finding algorithm, the lowest threshold being set to 3σ (red contours), and overlaid on the Hα image of the LMC (Kim et al 1999). The black box indicates the observed region in the Science Demonstration Program of Herschel Space Observatory (Meixner et al 2010).…”

Section: Physical Properties Of Dust Clumpsmentioning

confidence: 99%

Cold dust clumps in dynamically hot gas

Kim¹,

Kwon²,

Madden

et al. 2010

A&A

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Aims. We present clumps of dust emission from Herschel observations of the Large Magellanic Cloud (LMC) and their physical and statistical properties. We catalog cloud features seen in the dust emission from Herschel observations of the LMC, the Magellanic type irregular galaxy closest to the Milky Way, and compare these features with H i catalogs from the ATCA+Parkes H i survey.Methods. Using an automated cloud-finding algorithm, we identify clouds and clumps of dust emission and examine the cumulative mass distribution of the detected dust clouds. The mass of cold dust is determined from physical parameters that we derive by performing spectral energy distribution fits to 250, 350, and 500 μm emission from SPIRE observations using dust grain size distributions for graphite/silicate in low-metallicity extragalactic environments. Results. The dust cloud mass spectrum follows a power law distribution with an exponent of γ = −1.8 for clumps larger than 4 × 10 2 M and is similar to the H i mass distribution. This is expected from the theory of ISM structure in the vicinity of star formation.

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H [CSC]i[/CSC] Shells in the Large Magellanic Cloud

Cited by 243 publications

References 28 publications

OB stellar associations in the Large Magellanic Cloud: Survey of young stellar systems

OB stellar associations in the Large Magellanic Cloud: Survey of young stellar systems

The population of X-ray supernova remnants in the Large Magellanic Cloud

Cold dust clumps in dynamically hot gas

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