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Journal articles on the topic 'Large magellanic cloud'

Author: Grafiati
Published: 4 June 2021
Last updated: 15 February 2022

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1

Kim, S. "HI clouds in the Large Magellanic Cloud." Proceedings of the International Astronomical Union 2, S237 (August 2006): 434. http://dx.doi.org/10.1017/s1743921307002220.

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2

Brocato, E., E. Di Carlo, and G. Menna. "Large Magellanic Cloud stellar clusters." Astronomy & Astrophysics 374, no. 2 (August 2001): 523–39. http://dx.doi.org/10.1051/0004-6361:20010711.

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3

Evans, N. Wyn, and Eamonn Kerins. "Is the Large Magellanic Cloud a Large Microlensing Cloud?" Astrophysical Journal 529, no. 2 (February 2000): 917–24. http://dx.doi.org/10.1086/308328.

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4

Niemela, Virpi S. "Two New Massive Binary Stars in the Magellanic Clouds." Symposium - International Astronomical Union 207 (2002): 202–4. http://dx.doi.org/10.1017/s0074180900223759.

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The discovery and preliminary spectroscopic orbits of two early O type binaries in very young open clusters in the Magellanic Clouds is reported. The binaries are NGC 346–1 in the Small Magellanic Cloud, and HDE 270145 in NGC 2122 in the Large Magellanic Cloud.
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5

Yoshizawa, A. M., and M. Noguchi. "N-Body Simulations of the Magellanic System Including Gas Dynamics and Star Formation." Symposium - International Astronomical Union 186 (1999): 60. http://dx.doi.org/10.1017/s0074180900112276.

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The system of the Magellanic Clouds is considered to be dynamically interacting among themselves and with our Galaxy. This interaction is thought to be the cause of many complicated features seen in the Magellanic Clouds and the Magellanic Stream (see Westerlund 1990, A&AR, 2, 27). In order to better understand the formation and evolution of the Magellanic System, we carry out realistic N-body simulations of the tidal distortion of the Small Magellanic Cloud (SMC) due to our Galaxy and the Large Magellanic Cloud (LMC).
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6

Wong, Tony, Annie Hughes, Jürgen Ott, Jorge L. Pineda, and Erik Muller. "The Molecular Cloud Population of the Large Magellanic Cloud." Proceedings of the International Astronomical Union 8, S292 (August 2012): 71–74. http://dx.doi.org/10.1017/s1743921313000495.

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AbstractWe have mapped an extensive sample of molecular clouds in the Large Magellanic Cloud (LMC) at 11 pc resolution in the CO(1-0) line as part of the Magellanic Mopra Assessment (MAGMA). We identify clouds as regions of connected CO emission and determine their sizes, line widths, and fluxes. We find that GMCs are not preferentially located in regions of high Hi line width or velocity gradient, and that there is no clear Hi column density threshold for CO detection. The luminosity function of CO clouds is steeper than dN/dL ∝ L−2, suggesting a substantial fraction of mass in low-mass clouds. The correlation between size and linewidth, while apparent for the largest emission structures, breaks down when those structures are decomposed into smaller structures. The virial parameter (the ratio of a cloud's kinetic to gravitational energy) shows a wide range of values and exhibits no clear trends with the likelihood of hosting young stellar object (YSO) candidates, suggesting that this parameter is a poor reflection of the evolutionary state of a cloud. More massive GMCs are more likely to harbor a YSO candidate, and more luminous YSOs are more likely to be coincident with detectable CO emission, confirming GMCs as the principal sites of massive star formation.
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7

Youssoufi, Dalal El, Maria-Rosa L. Cioni, Cameron P. M. Bell, Stefano Rubele, Florian Niederhofer, and Gal Matijevic. "Morphology of stellar populations in the Magellanic Clouds using the VMC survey." Proceedings of the International Astronomical Union 14, S344 (August 2018): 66–69. http://dx.doi.org/10.1017/s1743921318006907.

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AbstractThe Magellanic Clouds are nearby dwarf irregular galaxies that represent a unique laboratory for studying galaxy interactions. Their morphology and dynamics have been heavily influenced by their mutual interactions as well as with their interaction(s) with the Milky Way. We use the VISTA near-infrared YJKs survey of the Magellanic Clouds system (VMC) in combination with stellar partial models of the Large Magellanic Cloud (LMC), the Small Magellanic Cloud (SMC) and the Milky Way to investigate the spatial distribution of stellar populations of different ages across the Magellanic Clouds. In this contribution, we present the results of these studies that allow us to trace substructures possibly related to the interaction history of the Magellanic Clouds.
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8

Rubio, Monica. "Molecular gas in the Small Magellanic Cloud." Symposium - International Astronomical Union 148 (1991): 429–30. http://dx.doi.org/10.1017/s007418090020106x.

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We summarize the results of observations of molecular gas from the Small Magellanic Cloud (SMC) made with low angular resolution (8'.8). These observations show that the CO emission is weak (TA˜ 0.04K) and that the CO luminosities of the Clouds are low compared to those of Galactic molecular clouds. The factor to convert the CO luminosity to molecular hydrogen column density for the SMC is ˜20 and three times larger than those derived for clouds in our Galaxy and in the Large Magellanic Cloud (LMC) respectively. In addition, we present preliminary results of high resolution (40″) observations of SMC molecular clouds made with the SEST telescope.
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9

Popowski, Piotr. "The Distance to the Large Magellanic Cloud." International Astronomical Union Colloquium 176 (2000): 203–7. http://dx.doi.org/10.1017/s0252921100057547.

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AbstractI demonstrate that the two unexpected results in the local Universe: anomalous intrinsic (V – I)0 colors of RR Lyrae stars and clump giants in the Galactic center, and very short distances to Magellanic Clouds inferred from clump giants, can be at least partially resolved with a modified coefficient of selective extinction AV/E(V – I). With this modification, I find a new clump-giant distance modulus to the Large Magellanic Cloud, μLMC = 18.27 ± 0.07, which is 0.09 larger than the Udalski (1998b) result. When distance estimates from the red clump, RR Lyrae stars and the eclipsing binary HV2274 are combined, one obtains μLMC = 18.31 ± 0.04 (internal).
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10

Ehrenfreund, P., N. Cox, J. Cami, B. H. Foing, L. Kaper, L. d’Hendecourt, J. P. Maier, et al. "Magellanic Diffuse Interstellar Bands and Carbon Chemistry." Highlights of Astronomy 13 (2005): 864–66. http://dx.doi.org/10.1017/s1539299600017342.

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AbstractWith the Ultraviolet Visual Echelle Spectrograph mounted at the Very Large Telescope, we have observed at unprecedented spectral resolution the absorption spectrum toward reddened stars in the Magellanic Clouds over the wavelength range of 3500-10500 Å. This range covers the strong transitions associated with neutral and charged large carbon molecules of varying sizes and structures. We report the first detection of diffuse interstellar bands (DIBs) at 5780 and 5797 Å in the Small Magellanic Cloud and the variation of those DIBs toward several targets in the Large Magellanic Cloud. The variation of DIBs in the Magellanic Clouds compared with Galactic targets may be governed by a combination of the different chemical processes prevailing in low-metallicity regions and the local environmental conditions. The analysis of high-resolution absorption spectra allows us to reveal the global effects in the chemistry and recycling of cosmic dust in the Magellanic Clouds which are relevant for the chemical pathways forming large organic molecules in external galaxies.
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11

Filipović, Miroslav D., Paul A. Jones, Graeme L. White, and Raymond F. Haynes. "Comparison of Discrete Sources in Radio and Hα Surveys of the Magellanic Clouds and the Potential for the New Hα Survey." Publications of the Astronomical Society of Australia 15, no. 1 (1998): 128–31. http://dx.doi.org/10.1071/as98128.

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AbstractWe present a comparison between the latest Parkes radio surveys (Filipović et al. 1995, 1996, 1997) and Hα surveys of the Magellanic Clouds (Kennicutt & Hodge 1986). We have found 180 discrete sources in common for the Large Magellanic Cloud (LMC) and 40 in the field of the Small Magellanic Cloud (SMC). Most of these sources (95%) are HII regions and supernova remnants (SNRs). A comparison of the radio and Hα flux densities shows a very good correlation and we note that many of the Magellanic Clouds SNRs are embedded in HII regions.
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12

van den Bergh, Sidney. "The Magellanic Clouds, Past, Present and Future - A Summary of IAU Symposium No. 190." Symposium - International Astronomical Union 190 (1999): 569–78. http://dx.doi.org/10.1017/s0074180900118856.

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Important problems to which we would like to find answers are: •What are the distances to the Large Magellanic Cloud (LMC) and the Small Magellanic Cloud (SMC)?•What is the present distribution of stars, gas and dark matter in the Clouds, and how did it evolve?•How, and where, did the Magellanic Clouds form, and how have their orbits evolved?•Finally the recent discovery of numerous microlensing events in the Clouds provides answers to questions that we have only recently started to ask.
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13

van den Bergh, Sidney. "The Magellanic Clouds, Past, Present and Future - A Summary of IAU Symposium No. 190." Symposium - International Astronomical Union 190 (1999): 569–78. http://dx.doi.org/10.1017/s0074180900119023.

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Important problems to which we would like to find answers are:•What are the distances to the Large Magellanic Cloud (LMC) and the Small Magellanic Cloud (SMC)?•What is the present distribution of stars, gas and dark matter in the Clouds, and how did it evolve?•How, and where, did the Magellanic Clouds form, and how have their orbits evolved?•Finally the recent discovery of numerous microlensing events in the Clouds provides answers to questions that we have only recently started to ask.
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14

van den Bergh, S. "Star clusters in the Magellanic Clouds." Symposium - International Astronomical Union 148 (1991): 161–64. http://dx.doi.org/10.1017/s0074180900200259.

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Star clusters in the Magellanic Clouds (MCs) differ from those in the Galaxy in a number of respects: (1) the Clouds contain a class of populous open clusters that has no Galactic counterpart; (2) Cloud clusters have systematically larger radii rh than those in the Galaxy; (3) clusters of all ages in the Clouds are, on average, more flattened than those in the Galaxy. In the Large Magellanic Cloud (LMC) there appear to have been two distinct epochs of cluster formation. LMC globulars have ages of 12-15 Gyr, whereas most populous open clusters have ages <5 Gyr. No such dichotomy is observed for clusters in the Small Magellanic Cloud (SMC) The fact that the SMC exhibits no enhanced cluster formation at times of bursts of cluster formation in the LMC, militates against encounters between the Clouds as a cause for enhanced rates of star and cluster formation.
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15

Priyatikanto, Rhorom, Mochamad Ikbal Arifyanto, Rendy Darma, Aprilia, and Muhamad Irfan Hakim. "Formation History of Binary Clusters in the Large Magellanic Cloud." Proceedings of the International Astronomical Union 14, S344 (August 2018): 118–21. http://dx.doi.org/10.1017/s1743921318005215.

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AbstractGlobal history of star or cluster formation in the Large Magellanic Cloud (LMC) has been the center of interest in several studies as it is thought to be influenced by tidal interaction with the Small Magellanic Cloud and even the Milky Way. This study focus on the formation history of the LMC in relation with the context of binary star clusters population, the apparent binary fraction (e.g., percentage of cluster pairs) in different epoch were calculated and analyzed. From the established distributions, it can be deduced that the binary clusters tend to be young (∽ 100 Myr) while their locations coincide with the locations of star forming complexes. There is an indication that the binary fraction increases as the rise of star formation rate in the last millions years. In the LMC, the increase of binary fraction at age ∽ 100 Myr can be associated to the last episode of close encounter with the Small Magellanic Cloud at ∽ 150 Myr ago. This observational evidence supports the theory of binary cluster formation through the fission of molecular cloud where the encounter between galaxies enhanced the clouds velocity dispersion which in turn increased the probability of cloud-cloud collisions that produce binary clusters.
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16

Gurwell, Mark, and Paul Hodge. "Galaxies behind the Large Magellanic Cloud." Publications of the Astronomical Society of the Pacific 102 (August 1990): 849. http://dx.doi.org/10.1086/132709.

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17

Imara, Nia, and Leo Blitz. "Extinction in the Large Magellanic Cloud." Astrophysical Journal 662, no. 2 (June 20, 2007): 969–79. http://dx.doi.org/10.1086/517911.

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18

Jetzer, Ph, L. Mancini, and G. Scarpetta. "Microlensing towards the Large Magellanic Cloud." Astronomy & Astrophysics 393, no. 1 (September 18, 2002): 129–47. http://dx.doi.org/10.1051/0004-6361:20021027.

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19

Fiorentino, G., E. Tolstoy, E. Diolaiti, E. Valenti, M. Cignoni, and A. D. Mackey. "MAD about the Large Magellanic Cloud." Astronomy & Astrophysics 535 (November 2011): A63. http://dx.doi.org/10.1051/0004-6361/201016094.

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20

Bertelli, Gianpaolo, Alessandro Bressan, Cesare Chiosi, Mario Mateo, and Peter R. Wood. "The distance to the Large Magellanic Cloud - Constraints from Cepheids in Large Magellanic Cloud star clusters." Astrophysical Journal 412 (July 1993): 160. http://dx.doi.org/10.1086/172908.

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21

Romita, Krista, Elizabeth Lada, and Maria-Rosa Cioni. "EMBEDDED CLUSTERS IN THE LARGE MAGELLANIC CLOUD USING THE VISTA MAGELLANIC CLOUDS SURVEY." Astrophysical Journal 821, no. 1 (April 11, 2016): 51. http://dx.doi.org/10.3847/0004-637x/821/1/51.

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22

Olsen, Knut A. G., Dennis Zaritsky, Robert D. Blum, Martha L. Boyer, and Karl D. Gordon. "A POPULATION OF ACCRETED SMALL MAGELLANIC CLOUD STARS IN THE LARGE MAGELLANIC CLOUD." Astrophysical Journal 737, no. 1 (July 26, 2011): 29. http://dx.doi.org/10.1088/0004-637x/737/1/29.

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23

Ruiz-Lara, T., C. Gallart, M. Monelli, D. Nidever, A. Dorta, Y. Choi, K. Olsen, et al. "The Large Magellanic Cloud stellar content with SMASH." Astronomy & Astrophysics 639 (July 2020): L3. http://dx.doi.org/10.1051/0004-6361/202038392.

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The Large Magellanic Cloud (LMC) is the closest and most studied example of an irregular galaxy. Among its principal defining morphological features, its off-centred bar and single spiral arm stand out, defining a whole family of galaxies known as the Magellanic spirals (Sm). These structures are thought to be triggered by tidal interactions and possibly maintained via gas accretion. However, it is still unknown whether they are long-lived stable structures. In this work, by combining photometry that reaches down to the oldest main sequence turn-off in the colour-magnitude diagrams (CMD, up to a distance of ∼4.4 kpc from the LMC centre) from the SMASH survey and CMD fitting techniques, we find compelling evidence supporting the long-term stability of the LMC spiral arm, dating the origin of this structure to more than 2 Gyr ago. The evidence suggests that the close encounter between the LMC and the Small Magellanic Cloud (SMC) that produced the gaseous Magellanic Stream and its Leading Arm also triggered the formation of the LMC’s spiral arm. Given the mass difference between the Clouds and the notable consequences of this interaction, we can speculate that this should have been one of their closest encounters. These results set important constraints on the timing of LMC-SMC collisions, as well as on the physics behind star formation induced by tidal encounters.
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24

Klein, U., R. F. Haynes, R. Wielebinski, S. R. Wayte, J. I. Harnett, E. Bajaja, J. D. Murray, et al. "Radio continuum emission from the Magellanic Clouds." Symposium - International Astronomical Union 148 (1991): 31–35. http://dx.doi.org/10.1017/s0074180900199966.

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New radio continuum surveys of the Large and the Small Magellanic Cloud have been completed recently at four frequencies, using the Parkes 64-m telescope. Here we shall discuss briefly the overall radio morphology of the Clouds at different frequencies and discuss the detected linear polarization. A preliminary integrated radio continuum spectrum of the Large Magellanic Cloud is also presented. Various aspects of future studies will be outlined.
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25

Haynes, R. F., S. Wayte, J. I. Harnett, U. Klein, R. Wielebinski, U. R. Buczilowski, E. Bajaja, et al. "Polarization in the Magellanic Clouds." Publications of the Astronomical Society of Australia 8, no. 04 (1990): 339–42. http://dx.doi.org/10.1017/s1323358000023687.

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AbstractWe present preliminary results from a number of deep radio polarization surveys being made of the Magellanic Clouds at 2.3 GHz, 4.75 GHz and 8.55 GHz. Extended and linearly polarized radio emission has been found at 2.3 and 4.75 GHz from both the Large Magellanic Cloud (LMC) and the Small Magellanic Cloud (SMC). However, as the analysis of these data is not yet complete we present only some of the 4.75 GHz results at this time.
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26

Niemela, Virpi S. "Massive Binaries in the Magellanic Clouds." Highlights of Astronomy 13 (2005): 463. http://dx.doi.org/10.1017/s1539299600016270.

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We present results of our ongoing observing program on search and studies of massive stars (O and WR type) in binary systems in our neighbor galaxies, the Magellanic Clouds. Radial velocity orbits are presented for two new binaries, one in the Small Magellanic Cloud and another in the Large Magellanic Cloud, and improved orbits for previously known systems. We compare orbital parameters of selected binaries containing O and WR type components. We also discuss the present status of knowledge for massive binary stars in the Magellanic Clouds and the problems encountered in their orbital studies such as stellar winds the ubiquitous tendency to be born in multiple systems.
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27

Gładkowski, Marcin, Marcin Hajduk, and Igor Soszyński. "Search for binary central stars of the Magellanic Clouds PNe." Proceedings of the International Astronomical Union 12, S323 (October 2016): 384–85. http://dx.doi.org/10.1017/s1743921317001892.

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AbstractThe Optical Gravitational Experiment (OGLE) was effectively used in discovering binary central stars of planetary nebulae (CSPNe). About 50 binary CSPNe have been hitherto identified in the Galaxy, almost half of them were detected in the OGLE database. We used the OGLE data to search for binary CSPNe in the Magellanic Clouds. We also searched for PNe mimics and removed them from the PNe sample. Here, we present results of the photometric analysis for Small Magellanic Cloud (SMC) and our progress on search of binary central stars in the Large Magellanic Cloud (LMC). So far, we have discovered one binary central star of the PN beyond the Milky Way, which is located in the Small Magellanic Cloud.
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28

Andrievsky, S. M., V. V. Kovtyukh, S. A. Korotin, M. Spite, and F. Spite. "Magellanic Clouds elemental abundances from F supergiants: Revisited results for the Large Magellanic Cloud." Astronomy & Astrophysics 367, no. 2 (February 2001): 605–12. http://dx.doi.org/10.1051/0004-6361:20000407.

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29

Zaritsky, Dennis, Jason Harris, Ian B. Thompson, and Eva K. Grebel. "The Magellanic Clouds Photometric Survey: The Large Magellanic Cloud Stellar Catalog and Extinction Map." Astronomical Journal 128, no. 4 (October 2004): 1606–14. http://dx.doi.org/10.1086/423910.

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30

De Boer, Klaas S. "The interstellar medium of the Magellanic Clouds from absorption lines." Symposium - International Astronomical Union 148 (1991): 401–6. http://dx.doi.org/10.1017/s0074180900201022.

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General aspects of ISM studies using absorption line studies are given and available data are reviewed. Topics are: galactic foreground gas, individual fields in the Magellanic Clouds (MCs) and MC coronae. Overall investigations are discussed. It is demonstrated that the metals in the gas of the Large Magellanic Cloud (LMC) and Small Magellanic Cloud (SMC) are a factor of 3 and 10, respectively, in abundance below solar levels. The depletion pattern in the LMC is similar to that of the Milky Way.
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31

Gouliermis, Dimitrios A. "The sub-solar initial mass function in the Large Magellanic Cloud." Proceedings of the International Astronomical Union 4, S256 (July 2008): 250–55. http://dx.doi.org/10.1017/s1743921308028524.

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AbstractThe 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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32

Wilcots, Eric M. "Magellanic type galaxies throughout the Universe." Proceedings of the International Astronomical Union 4, S256 (July 2008): 461–72. http://dx.doi.org/10.1017/s1743921308028871.

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AbstractThe Magellanic Clouds are often characterized as “irregular” galaxies, a term that implies an overall lack of organized structure. While this may be a fitting description of the Small Cloud, the Large Magellanic Cloud, contrary to popular opinion, should not be considered an irregular galaxy. It is characterized by a distinctive morphology of having an offset stellar bar and single spiral arm. Such morphology is relatively common in galaxies of similar mass throughout the local Universe, although explaining the origin of these features has proven challenging. Through a number of recent studies we are beginning to get a better grasp on what it means to be a Magellanic spiral. One key result of these works is that we now recognize that the most unique aspect of the Magellanic Clouds is not their structure, but, rather, their proximity to a larger spiral such as the Milky Way.
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33

Fujimoto, M., T. Sawa, and Y. Kumai. "The Magellanic Stream and the Magellanic Cloud System." Symposium - International Astronomical Union 186 (1999): 31–38. http://dx.doi.org/10.1017/s0074180900112161.

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A tidal model has been introduced to the triple system of the Galaxy, Large and Small Magellanic Clouds (the LMC and SMC hereafter) and successfully reproduced the Magellanic Stream (Murai and Fujimoto 1980; Lin and Lynden-Bell 1982; Gardiner et al. 1994; Gardiner and Noguchi 1995; Lin et al. 1995), a narrow band of diffuse atomic hydrogen gas emerging from the SMC region, passing by the South Galactic Pole along an overhead great circle spanning over 100° (Wannier and Wrixon 1972; Mathewson et al. 1974). The LMC and SMC have a hydrogen bridge and common envelope (Hindman 1964; McGee and Milton 1966) and, therefore, we can consider that they have been in a binary state for the Hubble time, revolving together around the Galaxy with a halo whose mass is larger than 1012M⊙ if the flat rotation curve extends up to more than 100 kpc. The strong gravitational force due to this heavy halo attracts the Magellanic Stream and produces the high negative radial velocities (Murai and Fujimoto 1980).
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34

Bekki, Kenji, Warrick J. Couch, Duncan A. Forbes, and M. A. Beasley. "Formation of Star Clusters in the LMC and SMC." Highlights of Astronomy 13 (2005): 198. http://dx.doi.org/10.1017/s1539299600015641.

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AbstractWe demonstrate that single and binary star clusters can be formed during cloud-cloud collisions triggered by the tidal interaction between the Large and Small Magellanic clouds. We run two different sets of self-consistent numerical simulations which show that compact, bound star clusters can be formed within the centers of two colliding clouds due to strong gaseous shocks, compression, and dissipation, providing the clouds have moderately large relative velocities (10 — 60 km s-1). The impact parameter determines whether the two colliding clouds become a single or a binary cluster. The star formation efficiency in the colliding clouds is dependent upon the initial ratio of the relative velocity of the clouds to the sound speed of the gas. Based on these results, we discuss the observed larger fraction of binary clusters, and star clusters with high ellipticity, in the Magellanic clouds.
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35

Harris, Jason, Dennis Zaritsky, Eva K. Grebel, and Ian Thompson. "Reconstructing the Star Formation History of the Magellanic Clouds." Symposium - International Astronomical Union 192 (1999): 72–78. http://dx.doi.org/10.1017/s0074180900203926.

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We are developing an algorithm to determine the star formation history (SFH) of a mixed stellar population. We will apply the algorithm to hundreds of regions in our Magellanic Clouds Photometric Survey data and reconstruct the spatially resolved star formation history of the Large Magellanic Cloud (LMC) and the Small Magellanic Cloud (SMC). In this paper, we demonstrate the algorithm on a typical region in the LMC, focussing on the obstacles and challenges facing us in attempting to reliably extract the SFH from photometric data.
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36

de Freitas Pacheco, J. A. "Evolutionary Models for the Magellanic Clouds. I. The Large Cloud." Astronomical Journal 116, no. 4 (October 1998): 1701–7. http://dx.doi.org/10.1086/300560.

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37

Siudek, M., A. Pollo, T. T. Takeuchi, Y. Ita, D. Kato, and T. Onaka. "Infrared composition of the Large Magellanic Cloud." Earth, Planets and Space 65, no. 3 (March 2013): 229–71. http://dx.doi.org/10.5047/eps.2012.09.001.

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38

Siudek, M., A. Pollo, T. T. Takeuchi, Y. Ita, D. Kato, and T. Onaka. "INFRARED COMPOSITION OF THE LARGE MAGELLANIC CLOUD." Publications of The Korean Astronomical Society 27, no. 4 (September 16, 2012): 223–24. http://dx.doi.org/10.5303/pkas.2012.27.4.223.

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39

Reid, Neill. "AGB evolution in the large magellanic cloud." Astrophysics and Space Science 156, no. 1-2 (1989): 73–79. http://dx.doi.org/10.1007/bf00646348.

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40

Michalska, G., and A. Pigulski. "Detached Binaries in the Large Magellanic Cloud." Highlights of Astronomy 13 (2005): 462. http://dx.doi.org/10.1017/s1539299600016269.

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Analysis of the radial-velocity and light curves of detached eclipsing binaries allows to derive stellar masses and radii and, in consequence, enables to find their distances. The method has been already applied to several LMC binaries, but in order to have the distance to the LMC determined with good accuracy, the parameters need to be known for a larger number of systems. As a first step we present results of the analysis of the photometry of over eighty detached binaries in the LMC selected from the OGLE-II catalog of 53 000 variable star candidates. If possible, we combine the OGLE-II data with the photometry from other projects (MACHO and EROS). As a result, we present the list of brightest eclipsing binaries in the LMC suitable for distance determination.
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41

Michalska, G., and A. Pigulski. "Detached binaries in the Large Magellanic Cloud." New Astronomy Reviews 48, no. 9 (July 2004): 719–25. http://dx.doi.org/10.1016/j.newar.2004.03.007.

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42

Laval, A., E. le Coarer, Y. P. Georgelin, M. Marcelin, P. Amram, G. Goldes, G. Carranza, and M. Rosado. "Hα Survey of the Large Magellanic Cloud." International Astronomical Union Colloquium 149 (1995): 155–59. http://dx.doi.org/10.1017/s0252921100022855.

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AbstractThe LMC is being surveyed in the Hα emission line with a scanning Fabry-Perot interferometer, attached to the 36 cm telescope of the Observatoire de Marseille. The present results concern the kinematical mapping of bright nebulae; it shows that the kinetic energy involved in the gas motion is closely related to the evolutionary stage of the embedded stars. In particular, in the 30 Dor nebula, a few one-peaked line profiles remain at the boundaries of the shells, among the numerous split areas. The 50-100 pc shells exhibit a relatively usual spherical expansion, with velocities in the same range at the boundaries. On the contrary, the 10-20 pc shells of the central core show different velocities of the one-peak sides of the shells.
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43

Tanvir, N. R., and A. Boyle. "Photometry of 40 Large Magellanic Cloud Cepheids." Monthly Notices of the Royal Astronomical Society 304, no. 4 (April 16, 1999): 957–60. http://dx.doi.org/10.1046/j.1365-8711.1999.02387.x.

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44

Garnett, D. R., J. R. Walsh, Y. H. Chu, and B. M. Lasker. "Bok Globules in the Large Magellanic Cloud." Astronomical Journal 117, no. 3 (March 1999): 1285–91. http://dx.doi.org/10.1086/300784.

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45

Reid, Neill. "Cocoon stars in the Large Magellanic Cloud." Astrophysical Journal 382 (November 1991): 143. http://dx.doi.org/10.1086/170703.

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46

Boreiko, R. T., and A. L. Betz. "Ionized carbon in the Large Magellanic Cloud." Astrophysical Journal 380 (October 1991): L27. http://dx.doi.org/10.1086/186165.

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47

Hatzidimitriou, D., D. H. Morgan, R. D. Cannon, and B. F. W. Croke. "Lithium in Large Magellanic Cloud carbon stars." Monthly Notices of the Royal Astronomical Society 341, no. 4 (June 1, 2003): 1290–98. http://dx.doi.org/10.1046/j.1365-8711.2003.06502.x.

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48

Reyniers, M., C. Abia, H. Van Winckel, T. Lloyd Evans, L. Decin, K. Eriksson, and K. R. Pollard. "AGB nucleosynthesis in the Large Magellanic Cloud." Astronomy & Astrophysics 461, no. 2 (October 9, 2006): 641–50. http://dx.doi.org/10.1051/0004-6361:20065893.

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49

Dickel, John R., and D. K. Milne. "Supernova Remnants in the Large Magellanic Cloud." Publications of the Astronomical Society of Australia 11, no. 2 (August 1994): 99–109. http://dx.doi.org/10.1017/s1323358000019780.

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AbstractTwelve supernova remnants in the Large Magellanic Cloud have now been observed with the Australia Telescope. These were all imaged in total intensity and where possible the linear polarisation was also mapped. In many respects this survey is similar to previous single-dish observations of Galactic supernova remnants, and comparisons are made with these results. Preliminary images are shown for several sources. The survey is continuing with additional array configurations and at other wavelengths.
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50

Feitzinger, J. V. "Star Formation in the Large Magellanic Cloud." Symposium - International Astronomical Union 115 (1987): 521–33. http://dx.doi.org/10.1017/s0074180900096315.

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Methods used in pattern recognition and cluster analysis are applied to investigate the spatial distribution of the star forming regions. The fractal dimension of these structures is deduced. The new 21 cm, radio continuum (1.4 GHz) and IRAS surveys reveal scale structures of 700 pc to 1500 pc being identical with the optically identified star forming sites. The morphological structures delineated by young stars reflect physical parameters which determine the star formation in this galaxy. The formation of spiral arm filaments is understandable by stochastic selfpropagating star formation processes.
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