The giant and supergiant shells of the Magellanic Clouds

Meaburn, J.

doi:10.1093/mnras/192.3.365

Cited by 258 publications

(232 citation statements)

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“…In addition to this feature, HV 5936 is located in a very different part of the LMC from our previous targets (see Fig. 1), lying several degrees north of the LMC's bar and superposed on a well-known '' hole '' in the LMC's H i distribution (McGee & Milton 1966), corresponding to the supergiant shell LMC 4 (Meaburn 1980). Its distance should reflect strongly the spatial orientation of the LMC, i.e., its inclination angle and line-of-nodes orientation, and could provide constraints on these factors.…”

Section: Introductionmentioning

confidence: 59%

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Fundamental Properties and Distances of Large Magellanic Cloud Eclipsing Binaries. IV. HV 5936

Fitzpatrick

Ribas

Guinan

et al. 2003

ApJ

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We have determined the fundamental properties and distance of a fourth eclipsing binary (EB) system in the Large Magellanic Cloud, HV 5936 ($B0.5 V + $B2 III). As in our previous studies, we combine '' classical '' EB light-curve and radial velocity curve analyses with modeling of the UV/optical spectral energy distribution of HV 5936 to produce a detailed characterization of the system. In this paper, we also include an analysis of the high-resolution optical absorption line spectra of the binary components. We find HV 5936 to be an Algol-class system, in which the masses of the primary and secondary stars have evolved via mass transfer to their current values of 11.6 and 4.7 M , respectively. The properties of the primary star are indistinguishable from those of a '' normal '' star of the same current mass. The secondary is found to be overluminous for its current mass and exhibits a factor of 2 enhancement in its surface He abundance. These results are compatible with case A mass exchange occurring during the core hydrogen-burning phase of the current secondary. The distance derived to the system, 43:2 AE 1:8 kpc, implies a distance of $44.3 kpc to the optical center of the LMC. This is several kiloparsecs closer than found in our analyses of other systems, and we suggest that HV 5936 lies '' above '' the LMC disk. This is supported by the very low interstellar H i column density and low E(BÀV ) found for the system-both of which are consistent with expected Milky Way foreground material-and may be associated with HV 5936's location near the LMC supergiant shell LMC 4.

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Section: Introductionmentioning

confidence: 59%

“…Its apparent location places it within the outlines of LMC 4, the largest supergiant H ii shell in the LMC (Goudis & Meaburn 1978;Meaburn 1980). The shell has a diameter of $1.1 kpc, and HV 5936 is positioned northeast of the shell center and near the inside edge.…”

mentioning

confidence: 96%

Fundamental Properties and Distances of Large Magellanic Cloud Eclipsing Binaries. IV. HV 5936

Fitzpatrick

Ribas

Guinan

et al. 2003

ApJ

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“…Using the rough sketch provided by Meaburn (1980) as a guide, we found structures which resembled their representation on the drawing. Some of these structures were difficult to locate, such as SGS 7, 8, and 9, because they are faint, incomplete and irregular.…”

Section: Methodsmentioning

confidence: 99%

Structure of Supergiant Shells in the Large Magellanic Cloud

Book

Chu

Gruendl

2008

ASTROPHYS J SUPPL S

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Nine supergiant shells (SGSs) have been identified in the Large Magellanic Cloud (LMC) based on H images, and 23 SGSs have been reported based on H i 21 cm line observations, but these sets do not always identify the same structures. We have examined the physical structure of the optically identified SGSs using H i channel maps and P-V diagrams to analyze the gas kinematics. There is good evidence for seven of the nine optically identified SGSs to be true shells. Of these seven H SGSs, four are the ionized inner walls of H i SGSs, while three are an ionized portion of a larger and more complex H i structure. All of the H SGSs are identified as such because they have OB associations along the periphery or in the center, with younger OB associations more often found along the periphery. After roughly 12 Myr, if no new OB associations have been formed, a SGS will cease to be identifiable at visible wavelengths. Thus, the presence and location of ionizing sources is the main distinction between shells seen only in H i and those also seen in H . Based on our analysis, H observations alone cannot unambiguously identify SGSs, especially in distant galaxies.

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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%

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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The giant and supergiant shells of the Magellanic Clouds

Cited by 258 publications

References 0 publications

Fundamental Properties and Distances of Large Magellanic Cloud Eclipsing Binaries. IV. HV 5936

Fundamental Properties and Distances of Large Magellanic Cloud Eclipsing Binaries. IV. HV 5936

Structure of Supergiant Shells in the Large Magellanic Cloud

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

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