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Relevant bibliographies by topics / Large magellanic cloud

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Academic literature on the topic 'Large magellanic cloud'

Author: Grafiati

Published: 4 June 2021

Last updated: 15 February 2022

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Journal articles on the topic "Large magellanic cloud"

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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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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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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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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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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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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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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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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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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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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Dissertations / Theses on the topic "Large magellanic cloud"

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Dirsch, Boris. "Chemical evolution in the large Magellanic cloud /." Aachen : Shaker, 2000. http://catalogue.bnf.fr/ark:/12148/cb37738870g.

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Abedigamba, Oyirwoth Patrick. "The structure of the Large Magellanic Cloud." Master's thesis, University of Cape Town, 2010. http://hdl.handle.net/11427/13514.

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Includes bibliographical references (leaves 67-69).
This work gives an account of the study of the metallicity [Fe/H] distribution (gradient) in the oldest population in the Large Magellanic Cloud (LMC), by making use of the available RR Lyrae data from the Optical Gravitational Lensing Experiment III (OGLE III). RR Lyrae stars are amongst the oldest objects in the universe and they have a range in element (metal) abundances. Measuring the distribution of metallicities of RR Lyrae stars in a galaxy gives one clues to the origin of galaxies. It is known that the pulsation periods of RR Lyraes is broadly correlated with their metallicity. This fact has been used for investigating the metallicity distribution of RR Lyrae stars in the LMC. I have found an indication that the proportion of metal poor RR Lyrae stars increases with distance from the centre of the LMC. In addition, an attempt was made to improve the metallicity-period relation by introducing the Fourier parameters, but this was unsuccessful. Lastly, a comparison is made with estimates of metallicity gradients of other LMC populations.

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Elson, R. A. W. "The rich star clusters in the Large Magellanic Cloud." Thesis, University of Cambridge, 1986. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.373672.

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Nidever, David L., Knut Olsen, Alistair R. Walker, A. Katherina Vivas, Robert D. Blum, Catherine Kaleida, Yumi Choi, et al. "SMASH: Survey of the MAgellanic Stellar History." IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/626050.

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The Large and Small Magellanic Clouds are unique local laboratories for studying the formation and evolution of small galaxies in exquisite detail. The Survey of the MAgellanic Stellar History (SMASH) is an NOAO community Dark Energy Camera (DECam) survey of the Clouds mapping 480 deg2 (distributed over similar to 2400 square degrees at similar to 20% filling factor) to similar to 24th. mag in ugriz. The primary goals of SMASH are to identify low surface brightness stellar populations associated with the stellar halos and tidal debris of the Clouds, and to derive spatially resolved star formation histories. Here, we present a summary of the survey, its data reduction, and a description of the first public Data Release (DR1). The SMASH DECam data have been reduced with a combination of the NOAO Community Pipeline, the PHOTRED automated point-spread-function photometry pipeline, and custom calibration software. The astrometric precision is similar to 15 mas and the accuracy is similar to 2 mas with respect to the Gaia reference frame. The photometric precision is similar to 0.5%-0.7% in griz and similar to 1% in u with a calibration accuracy of similar to 1.3% in all bands. The median 5s point source depths in ugriz are 23.9, 24.8, 24.5, 24.2, and 23.5 mag. The SMASH data have already been used to discover the Hydra II Milky Way satellite, the SMASH 1 old globular cluster likely associated with the LMC, and extended stellar populations around the LMC out to R. similar to. 18.4 kpc. SMASH DR1 contains measurements of similar to 100 million objects distributed in 61 fields. A prototype version of the NOAO Data Lab provides data access and exploration tools.

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Hatano, H., R. Kadowaki, D. Kato, S. Sato, and the IRSF/SIRIUS group. "IRSF/SIRIUS near-infrared survey of the Magellanic Clouds: triggered star formation in N11 in the Large Magellanic Cloud." Cambridge University Press, 2006. http://hdl.handle.net/2237/10293.

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Nishiuchi, Mamiko. "X-ray study of Hot Plasmas in the Large Magellanic Cloud in the Magellanic Clouds - evolution from supernova remnants toward interstellar matter." 京都大学 (Kyoto University), 2001. http://hdl.handle.net/2433/150823.

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Oey, Marion Siang-li. "The stellar content and dynamics of superbubbles in the Large Magellanic Cloud." Diss., The University of Arizona, 1995. http://hdl.handle.net/10150/187375.

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The interaction between massive stars and the ISM is a fundamental process determining the structure and composition of the ISM. This work examines the stellar content and resulting dynamics of superbubbles in the LMC. We first show analytically that for 2 single-O star bubbles in M33, the evolution of wind power as the stars evolve is important in the bubble evolution. In a second prototype study, we find that the LMC superbubble DEM 152 shows evidence for sequential star formation, based on differing ages between the stars interior and exterior to the shell. We construct a numerical form of the standard Weaver et al. (1977) evolutionary model for wind-driven bubbles, and use the stellar census to compare the predicted shell evolution with the observed kinematics. There is a substantial discrepancy: shell's observed expansion velocity too large relative to its radius. I then find that the CMDs of the associations within 7 LMC superbubbles and 5 classical H II regions are indistinguishable. The HRDs, constructed with spectral types for 6 superbubble clusters, also appear similar to those in classical H II regions, implying that the shell formation timescale is shorter than the cluster evolutionary timescale. The stellar winds of the 1-2 most massive stars must therefore dominate the shell formation. The star-forming events for the superbubble associations are also no more extended in duration than that of other OB associations. The IMF slopes appear normal. Numerical modeling of the 6 superbubbles shows results falling into two distinct categories: "high-velocity" objects showing anomalous kinematics like DEM 152 and "low-velocity" objects which appear fairly consistent with the model. X-ray evidence suggests that the high-velocity objects have been accelerated by SNR impacts. Results for both categories imply an overestimate in the growth rate equivalent to an effective input power of up to an order of magnitude too large. I find that the superbubbles are likely to be struck and "burst" by such SNR impacts if the prior stellar wind power is log L(w) ≲ 37.8 erg s⁻¹. The interior coronal gas is then expelled by the pressure differential with the environment, which could greatly enhance the dispersal and distribution of the hot ionized medium. A minority of superbubbles with stellar wind power above the threshold are more likely to grow to the sizes of supergiant shells.

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Neilson, Hilding R., Robert G. Izzard, Nobert Langer, and Richard Ignace. "The Strange Evolution of the Large Magellanic Cloud Cepheid OGLE-LMC-CEP1812." Digital Commons @ East Tennessee State University, 2015. https://dc.etsu.edu/etsu-works/2696.

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Classical Cepheids are key probes of both stellar astrophysics and cosmology as standard candles and pulsating variable stars. It is important to understand Cepheids in unprecedented detail in preparation for upcoming Gaia, James Webb Space Telescope (JWST) and extremely-large telescope observations. Cepheid eclipsing binary stars are ideal tools for achieving this goal, however there are currently only three known systems. One of those systems, OGLE-LMC-CEP1812, raises new questions about the evolution of classical Cepheids because of an apparent age discrepancy between the Cepheid and its red giant companion. We show that the Cepheid component is actually the product of a stellar merger of two main sequence stars that has since evolved across the Hertzsprung gap of the HR diagram. This post-merger product appears younger than the companion, hence the apparent age discrepancy is resolved. We discuss this idea and consequences for understanding Cepheid evolution.

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Olsen, Knut A. G. "The formation and evolution of the large magellanic cloud from selected clusters and star fields /." Thesis, Connect to this title online; UW restricted, 1998. http://hdl.handle.net/1773/5426.

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Muraveva, Tatiana <1986&gt. "Improving the cosmic distance ladder. Distance and structure of the Large Magellanic Cloud." Doctoral thesis, Alma Mater Studiorum - Università di Bologna, 2014. http://amsdottorato.unibo.it/6733/.

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The Large Magellanic Cloud (LMC) is widely considered as the first step of the cosmological distance ladder, since it contains many different distance indicators. An accurate determination of the distance to the LMC allows one to calibrate these distance indicators that are then used to measure the distance to far objects. The main goal of this thesis is to study the distance and structure of the LMC, as traced by different distance indicators. For these purposes three types of distance indicators were chosen: Classical Cepheids,``hot'' eclipsing binaries and RR Lyrae stars. These objects belong to different stellar populations tracing, in turn, different sub-structures of the LMC. The RR Lyrae stars (age >10 Gyr) are distributed smoothly and likely trace the halo of the LMC. Classical Cepheids are young objects (age 50-200 Myr), mainly located in the bar and spiral arm of the galaxy, while ``hot'' eclipsing binaries mainly trace the star forming regions of the LMC. Furthermore, we have chosen these distance indicators for our study, since the calibration of their zero-points is based on fundamental geometric methods. The ESA cornerstone mission Gaia, launched on 19 December 2013, will measure trigonometric parallaxes for one billion stars with an accuracy of 20 micro-arcsec at V=15 mag, and 200 micro-arcsec at V=20 mag, thus will allow us to calibrate the zero-points of Classical Cepheids, eclipsing binaries and RR Lyrae stars with an unprecedented precision.

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Books on the topic "Large magellanic cloud"

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Morel, Mati. A visual atlas of the Large Magellanic Cloud. 2nd ed. Rankin Park, N.S.W., Australia: [Morel Astrographics], 1991.

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End in fire: The supernova in the large magellanic cloud. Cambridge [England]: Cambridge University Press, 1990.

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Imshennik, V. S. Supernova 1987A in the large Magellanic Cloud: Observations and theory. Chur: Harwood Academic Publishers, 1989.

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Cassatella, A. Ultraviolet observations by the IUE of 31 clusters of large magellanic cloud. Madrid: IUE Observatory, 1986.

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Ortiz, Patricio F. A CCD BVRI photometric study of star clusters in the Large Magellanic Cloud. Toronto: University of Toronto, Dept. of Astronomy, 1992.

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Patterson, Timothy Graham. A survey of the Galactic Bulge,Large Magellanic Cloud and Cygnus region with a simple configuration coded mask X-ray telescope. Birmingham: University of Birmingham, 1990.

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C, Kafatos Minas, and Michalitsianos A. G, eds. Supernova 1987A in the Large Magellanic Cloud: Proceedings of the Fourth George Mason Astrophysics Workshop held at the George Mason University, Fairfax, Virginia, 12-14 October 1987. Cambridge [Cambridgeshire]: Cambridge University Press, 1988.

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Absorption of the X-ray background by the Large Magellanic Cloud. [Washington, DC: National Aeronautics and Space Administration, 1991.

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United States. National Aeronautics and Space Administration., ed. Absorption of the X-ray background by the Large Magellanic Cloud. [Washington, DC: National Aeronautics and Space Administration, 1991.

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Ortiz, Patricio Fredy. A CCD BVRI photometric study of star clusters in the large Magellanic Cloud. 1992.

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Book chapters on the topic "Large magellanic cloud"

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Chu, You-Hua, and Mordecai-Mark MacLow. "X-Rays from Superbubbles in the Large Magellanic Cloud." In The Magellanic Clouds, 99–100. Dordrecht: Springer Netherlands, 1991. http://dx.doi.org/10.1007/978-94-011-3432-3_18.

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Costa, M. E., P. M. McCulloch, and P. A. Hamilton. "The Magnetic Field Strength in the Large Magellanic Cloud." In The Magellanic Clouds, 101–2. Dordrecht: Springer Netherlands, 1991. http://dx.doi.org/10.1007/978-94-011-3432-3_19.

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Mateo, Mario, Douglas Welch, and Phil Fischer. "Mass to Light Ratios of Large Magellanic Cloud Clusters." In The Magellanic Clouds, 191–92. Dordrecht: Springer Netherlands, 1991. http://dx.doi.org/10.1007/978-94-011-3432-3_38.

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McCarthy, M. F., and V. M. Blanco. "Charting Cool Carbon Stars in the Large Magellanic Cloud." In The Magellanic Clouds, 353–54. Dordrecht: Springer Netherlands, 1991. http://dx.doi.org/10.1007/978-94-011-3432-3_88.

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Wood, P. R., M. S. Bessell, S. M. G. Hughes, A. R. Hyland, J. B. Whiteoak, F. F. Gardner, and R. E. Otrupcek. "OH/IR Stars in the Large Magellanic Cloud: The Observations." In The Magellanic Clouds, 386–87. Dordrecht: Springer Netherlands, 1991. http://dx.doi.org/10.1007/978-94-011-3432-3_103.

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Rohlfs, K., and Th Luks. "Hi-Distribution, Kinematics and Geometry of the Large Magellanic Cloud." In The Magellanic Clouds, 63–67. Dordrecht: Springer Netherlands, 1991. http://dx.doi.org/10.1007/978-94-011-3432-3_11.

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Feitzinger, J. V., and J. Spicker. "Turbulence and Stochastic Star Formation in the Large Magellanic Cloud." In The Magellanic Clouds, 103–4. Dordrecht: Springer Netherlands, 1991. http://dx.doi.org/10.1007/978-94-011-3432-3_20.

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Meaburn, J. "Studies of the Large Magellanic Cloud Using Optical Interstellar Emission Lines." In The Magellanic Clouds, 421–27. Dordrecht: Springer Netherlands, 1991. http://dx.doi.org/10.1007/978-94-011-3432-3_112.

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Reid, Neill, and Wendy L. Freedman. "A Survey for RR Lyrae Variables in the Large Magellanic Cloud." In The Magellanic Clouds, 365–66. Dordrecht: Springer Netherlands, 1991. http://dx.doi.org/10.1007/978-94-011-3432-3_93.

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Schommer, R. A. "The Kinematics and Abundances of Star Clusters in the Large Magellanic Cloud." In The Magellanic Clouds, 171–76. Dordrecht: Springer Netherlands, 1991. http://dx.doi.org/10.1007/978-94-011-3432-3_35.

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Conference papers on the topic "Large magellanic cloud"

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Komin, Nukri, Chia-Chun Lu, Michael Mayer, Stefan Ohm, Matthieu Renaud, and Jacco Vink. "H.E.S.S. Observations of the Large Magellanic Cloud." In The 34th International Cosmic Ray Conference. Trieste, Italy: Sissa Medialab, 2016. http://dx.doi.org/10.22323/1.236.0849.

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Tasitsiomi, Argyro. "Neutralino annihilation in the Large Magellanic Cloud." In HIGH ENERGY GAMMA-RAY ASTRONOMY: 2nd International Symposium on High Energy Gamma-Ray Astronomy. AIP, 2005. http://dx.doi.org/10.1063/1.1878442.

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Kim, Sungeun, and Lister Staveley-Smith. "The HI supergiant shells in the large Magellanic cloud." In The seventh astrophysical conference: Star formation, near and far. AIP, 1997. http://dx.doi.org/10.1063/1.52768.

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Dziembowski, W. A., R. Smolec, Joyce Ann Guzik, and Paul A. Bradley. "Multimode Cepheids in the Large Magellanic Cloud—challenges for theory." In STELLAR PULSATION: CHALLENGES FOR THEORY AND OBSERVATION: Proceedings of the International Conference. AIP, 2009. http://dx.doi.org/10.1063/1.3246580.

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Subramaniam, Annapurni. "The Parent Population of Novae in the Large Magellanic Cloud." In CLASSICAL NOVA EXPLOSIONS: International Conference on Classical Nova Explosions. AIP, 2002. http://dx.doi.org/10.1063/1.1518248.

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Komin, Nukri, and Maria Haupt. "Search for Point-Like Sources in the Large Magellanic Cloud." In 36th International Cosmic Ray Conference. Trieste, Italy: Sissa Medialab, 2020. http://dx.doi.org/10.22323/1.358.0716.

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Blair, William P., Cristina M. Oliveira, Stephanie M. LaMassa, Ravi Sankrit, Charles W. Danforth, Michael E. Van Steenberg, George Sonneborn, H. Warren Moos, and William P. Blair. "FUSE Observations of O VI Absorption in the Large Magellanic Cloud." In FUTURE DIRECTIONS IN ULTRAVIOLET SPECTROSCOPY: A Conference Inspired by the Accomplishments of the Far Ultraviolet Spectroscopic Explorer Mission. AIP, 2009. http://dx.doi.org/10.1063/1.3154081.

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Mancini, L. "Compact Dark Objects and Gravitational Microlensing towards the Large Magellanic Cloud." In HIGHLIGHTS IN CONDENSED MATTER PHYSICS. AIP, 2003. http://dx.doi.org/10.1063/1.1639602.

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Weidenspointner, G., V. Lonjou, and J. Knödlseder. "What can we learn from the Large Magellanic Cloud with GLAST?" In THE FIRST GLAST SYMPOSIUM. AIP, 2007. http://dx.doi.org/10.1063/1.2757420.

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Bernard-Salas, J. "Mid-IR Spectroscopy of Planetary Nebulae in the Large Magellanic Cloud." In PLANETARY NEBULAE AS ASTRONOMICAL TOOLS: International Conference on Planetary Nebulae as Astronomical Tools. AIP, 2005. http://dx.doi.org/10.1063/1.2146226.

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Reports on the topic "Large magellanic cloud"

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Alcock, C., R. A. Allsman, D. R. Alves, T. S. Axelrod, A. Basu, A. C. Becker, D. P. Bennett, et al. MACHO project 9 million star color-magnitude diagram of the large magellanic cloud. Office of Scientific and Technical Information (OSTI), January 2000. http://dx.doi.org/10.2172/15006433.

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