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Academic literature on the topic 'Magellanic Clouds'

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Published: 4 June 2021
Last updated: 8 June 2024

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Journal articles on the topic "Magellanic Clouds"

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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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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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Martin, F., and S. J. McCarthy. "Harlow Shapley and Red Giant Stars." Symposium - International Astronomical Union 126 (1988): 481–82. http://dx.doi.org/10.1017/s0074180900042716.

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In five papers written between 1951 and 1955 Shapley considers the topic of red giant stars and reddish variable stars in the Magellanic Clouds. These works coincide with Shapley's final year as Director at Harvard and the first years of his retirement which extended a full score of years before his death in 1972. They include the following: Magellanic Clouds II (Supergiants/Red Variable Stars in the Small Cloud; January 1951); Magellanic Clouds IV (On Period Frequency Anomalies; February 1952); Magellanic Clouds VII (Star Colors and Luminosities in Five Constellations; March 1953); Magellanic Clouds VIII (On the Populations Characteristics of the Two Clouds; October 1953); and Magellanic Clouds XVI (Infrared Stars and Stellar Evolution; July 1955). These five papers, which appeared originally in the Proceedings of the National Academy of Science, may be found in the Harvard Reprint Series I as numbers 346, 360, 373, 376, and 425.
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Reggiani, Henrique, Kevin C. Schlaufman, Andrew R. Casey, Joshua D. Simon, and Alexander P. Ji. "The Most Metal-poor Stars in the Magellanic Clouds Are r-process Enhanced*." Astronomical Journal 162, no. 6 (November 5, 2021): 229. http://dx.doi.org/10.3847/1538-3881/ac1f9a.

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Abstract The chemical abundances of a galaxy’s metal-poor stellar population can be used to investigate the earliest stages of its formation and chemical evolution. The Magellanic Clouds are the most massive of the Milky Way’s satellite galaxies and are thought to have evolved in isolation until their recent accretion by the Milky Way. Unlike the Milky Way’s less massive satellites, little is known about the Magellanic Clouds’ metal-poor stars. We have used the mid-infrared metal-poor star selection of Schlaufman & Casey and archival data to target nine LMC and four SMC giants for high-resolution Magellan/MIKE spectroscopy. These nine LMC giants with −2.4 ≲ [Fe/H] ≲ −1.5 and four SMC giants with −2.6 ≲ [Fe/H] ≲ −2.0 are the most metal-poor stars in the Magellanic Clouds yet subject to a comprehensive abundance analysis. While we find that at constant metallicity these stars are similar to Milky Way stars in their α, light, and iron-peak elemental abundances, both the LMC and SMC are enhanced relative to the Milky Way in the r-process element europium. These abundance offsets are highly significant, equivalent to 3.9σ for the LMC, 2.7σ for the SMC, and 5.0σ for the complete Magellanic Cloud sample. We propose that the r-process enhancement of the Magellanic Clouds’ metal-poor stellar population is a result of the Magellanic Clouds’ isolated chemical evolution and long history of accretion from the cosmic web combined with r-process nucleosynthesis on a timescale longer than the core-collapse supernova timescale but shorter than or comparable to the thermonuclear (i.e., Type Ia) supernova timescale.
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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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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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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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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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Ashley, Trisha, Andrew J. Fox, Felix J. Lockman, Bart P. Wakker, Philipp Richter, David M. French, Vanessa A. Moss, and Naomi M. McClure-Griffiths. "The Metallicities of Five Small High-velocity Clouds*." Astrophysical Journal 961, no. 1 (January 1, 2024): 94. http://dx.doi.org/10.3847/1538-4357/ad0cb7.

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Abstract High-velocity clouds (HVCs) are multiphase gas structures whose velocities (∣v LSR∣ ≥ 100 km s−1) are too high to be explained by Galactic disk rotation. While large HVCs are well characterized, compact and small HVCs (with H i angular sizes of a few degrees) are poorly understood. Possible origins for such small clouds include Milky Way (MW) halo gas or fragments of the Magellanic System, but neither their origin nor their connection to the MW halo has been confirmed. We use new Hubble Space Telescope/Cosmic Origins Spectrograph UV spectra and Green Bank Telescope H i spectra to measure the metallicities of five small HVCs in the southern Galactic sky projected near the Magellanic System. We build a set of distance-dependent Cloudy photoionization models for each cloud and calculate their ionization-corrected metallicities. All five small HVCs have oxygen metallicities ≤0.17 Z ⊙, indicating they do not originate in the disk of the MW. Two of the five have metallicities of 0.16–0.17 Z ⊙, similar to the Magellanic Stream, suggesting these clouds are fragments of the Magellanic System. The remaining three clouds have much lower metallicities of 0.02–0.04 Z ⊙. While the origin of these low-metallicity clouds is unclear, they could be gaseous minihalos or gas stripped from dwarf galaxies by ram pressure or tidal interactions. These results suggest that small HVCs do not all reside in the inner MW halo or the Magellanic System, but instead can trace more distant structures.
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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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Dissertations / Theses on the topic "Magellanic Clouds"

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Ye, Taisheng. "Nebulae in the Magellanic clouds." Thesis, The University of Sydney, 1988. https://hdl.handle.net/2123/26240.

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In this thesis I am primarily concerned with radio observations of the nebulae in the Magellanic Clouds, with particular emphasis on the regions of ionised gas in the Small Magellanic Cloud (SMC). Nebulae (Latin for ‘clouds’) are luminous fuzzy celestial objects with diverse size, shape and brightness. After several generations of observational and theoretical work, nebulae have been classified into four categories: external galaxies, H II regions, supernova remnants (SNRs) and planetary nebulae (PN). External galaxies are no longer regarded as true nebulae. H II regions are ionised hydrogen and are excited by the intense ultraviolet radiation of central or nearby hot stars. A planetary nebula is an extended, low density envelope which has expanded outward from a red giant star at a late stage in its evolution. SNRs are formed by the high velocity and high temperature material ejected when a star ends its life with a violent explosion. The current matters of interest in nebulae research concentrate on their classification and evolution, and their relation to the interstellar medium and to nucleosynthesis in their parent galaxies. Specifically, many investigations are directed toward the measurements of physical parameters such as electron temperature, density and elemental abundances, the morphologies of individual nebulae, spatial distributions of each type of nebula in galaxies, the number counts of sources within different luminosity ranges (the luminosity functions) and within different diameter ranges (diameter functions), the global absorption, scattering or reflection by dust (extinction) inside or outside of a nebula and the extinction distribution over a nebula.
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Danforth, Charles Weston. "Interstellar matter kinematics in the magellanic clouds." Available to US Hopkins community, 2003. http://wwwlib.umi.com/dissertations/dlnow/3080648.

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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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Hunter, Ian Kennedy. "Evolution of massive stars in the Magellanic clouds." Thesis, Queen's University Belfast, 2008. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.492010.

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Rotation and the associated mixing has recently been included in massive star evolutionary models in an attempt to reconcile theory with observation, e.g surface abundance anomalies, such as nitrogen enrichments. However, despite the apparent importance of rotation there have been few observational tests, specifically in regard to fast rotating stars. This thesis presents the analysis of the Magellanic Cloud B-type stars from the 'The VLT-FLAMES survey of massive stars'. Atmospheric paramaters and rotational velocities have been estimated for rv400 objects, with chemical compositions being derived for over half this sample. This represents the largest homogenous survey undertaken to date. Comparison of the rotational velocity distributions in the SMC, LMC and our Galaxy reveals that objects at low metallicity typically rotate faster as predicted. Additionally the velocity distributions imply that the end of the core-hydrogen burning phase needs to be extended in current theoretical models. The present-day chemical compositions of the Magellanic Clouds have been derived, demonstrating that simply scaling the solar composition is not appropriate for all elements. Additionally chemical compositions have been estimated for a broad range of rotational velocities and hence are ideal for exploring the theory of rotational mixing. In the SMC and LMC both an excess of nitrogen enriched core hydrogen burning slowly rotating objects and highly enriched supergiants are observed. Additionally a group of LMC objects near the end of core-hydrogen burning with large rotational velocities and little enrichment has been identified. These observations are all incompatible with currently adopted rotational mixing theories. The work in this thesis highlights the need for examining entire populations of objects in order to make meaningful and robust comparisons with theory as well as providing a significant advance in our knowledge of massive star evolution.
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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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Bitsakis, Theodoros, R. A. González-Lópezlira, P. Bonfini, G. Bruzual, G. Maravelias, D. Zaritsky, S. Charlot, and V. H. Ramírez-Siordia. "The Distribution and Ages of Star Clusters in the Small Magellanic Cloud: Constraints on the Interaction History of the Magellanic Clouds." IOP PUBLISHING LTD, 2018. http://hdl.handle.net/10150/626531.

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We present a new study of the spatial distribution and ages of the star clusters in the Small Magellanic Cloud (SMC). To detect and estimate the ages of the star clusters we rely on the new fully automated method developed by Bitsakis et al. Our code detects 1319 star clusters in the central 18 deg(2) of the SMC we surveyed (1108 of which have never been reported before). The age distribution of those clusters suggests enhanced cluster formation around 240 Myr ago. It also implies significant differences in the cluster distribution of the bar with respect to the rest of the galaxy, with the younger clusters being predominantly located in the bar. Having used the same setup, and data from the same surveys as for our previous study of the LMC, we are able to robustly compare the cluster properties between the two galaxies. Our results suggest that the bulk of the clusters in both galaxies were formed approximately 300 Myr ago, probably during a direct collision between the two galaxies. On the other hand, the locations of the young (<= 50 Myr) clusters in both Magellanic Clouds, found where their bars join the H I arms, suggest that cluster formation in those regions is a result of internal dynamical processes. Finally, we discuss the potential causes of the apparent outside-in quenching of cluster formation that we observe in the SMC. Our findings are consistent with an evolutionary scheme where the interactions between the Magellanic Clouds constitute the major mechanism driving their overall evolution.
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Rolleston, William Robert James. "Young stars in Galactic clusters and the Magellanic Clouds." Thesis, Queen's University Belfast, 1994. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.282334.

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Amy, Shaun Wallace. "A Radio Study of Selected Regions in the Magellanic Clouds." Thesis, The University of Sydney, 2000. http://hdl.handle.net/2123/358.

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The Magellanic Clouds have long provided a rich celestial laboratory for many astrophysical research programmes. Their location relatively close to the Earth and away from the plane of our Galaxy has made them a natural target for Southern Hemisphere ground-based instrumentation. Likewise, the continuing quest for images of the Clouds with higher dynamic range and improved angular resolution has driven a continual improvement in instrumentation across a range of wavelength bands. The cornerstone of this thesis is a study of selected sources in the Magellanic Clouds. The sample was chosen from the 843MHz Molonglo Observatory Synthesis Telescope survey of the Clouds, based on the existing knowledge of each source, its flux density and angular extent. This sample was used to explore observational and analysis techniques with the Australia Telescope Compact Array in order to better determine the nature of these objects and to identify those sources worthy of further study. This work highlights many pertinent issues associated with the correct classification of sources when only a limited amount of data is available. These issues led directly to the development of a more systematic approach in the classification of the Large Magellanic Cloud source sample, detailed for the first time in this thesis. Two supernova remnants in the Small Magellanic Cloud were studied in detail. The Australia Telescope images of 1E0102.2-7219 revealed, for the first time, the radio structure of this young oxygen-rich supernova remnant, and allowed a detailed comparison with existing optical and X-ray data to be undertaken. The comparisons presented in this thesis and in an earlier publication have prompted exciting new X-ray observations at unprecedented angular resolution. The second, 0101-7226, studied as part of an international collaboration, has a shell morphology at radio wavelengths but no associated X-ray emission and is therefore something of an enigma.
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Amy, Shaun Wallace. "A Radio Study of Selected Regions in the Magellanic Clouds." University of Sydney. Physics, 2000. http://hdl.handle.net/2123/358.

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The Magellanic Clouds have long provided a rich celestial laboratory for many astrophysical research programmes. Their location relatively close to the Earth and away from the plane of our Galaxy has made them a natural target for Southern Hemisphere ground-based instrumentation. Likewise, the continuing quest for images of the Clouds with higher dynamic range and improved angular resolution has driven a continual improvement in instrumentation across a range of wavelength bands. The cornerstone of this thesis is a study of selected sources in the Magellanic Clouds. The sample was chosen from the 843MHz Molonglo Observatory Synthesis Telescope survey of the Clouds, based on the existing knowledge of each source, its flux density and angular extent. This sample was used to explore observational and analysis techniques with the Australia Telescope Compact Array in order to better determine the nature of these objects and to identify those sources worthy of further study. This work highlights many pertinent issues associated with the correct classification of sources when only a limited amount of data is available. These issues led directly to the development of a more systematic approach in the classification of the Large Magellanic Cloud source sample, detailed for the first time in this thesis. Two supernova remnants in the Small Magellanic Cloud were studied in detail. The Australia Telescope images of 1E0102.2-7219 revealed, for the first time, the radio structure of this young oxygen-rich supernova remnant, and allowed a detailed comparison with existing optical and X-ray data to be undertaken. The comparisons presented in this thesis and in an earlier publication have prompted exciting new X-ray observations at unprecedented angular resolution. The second, 0101-7226, studied as part of an international collaboration, has a shell morphology at radio wavelengths but no associated X-ray emission and is therefore something of an enigma.
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Stanimirović, Snežana. "The complex nature of the ISM in the SMC : an HI and infrared study /." View thesis, 1999. http://library.uws.edu.au/adt-NUWS/public/adt-NUWS20030826.143835/index.html.

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Thesis (PhD) -- University of Western Sydney, Nepean, 1999.
"A thesis submitted for the degree of Doctor of Philosophy at the University of Western Sydney Nepean" "July, 1999" Bibliography : p. 177-185.
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Books on the topic "Magellanic Clouds"

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Haynes, Raymond, and Douglas Milne, eds. The Magellanic Clouds. Dordrecht: Springer Netherlands, 1991. http://dx.doi.org/10.1007/978-94-011-3432-3.

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Westerlund, Bengt E. The Magellanic Clouds. Cambridge: Cambridge University Press, 1997.

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

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1944-, Haynes Raymond, and Milne Douglas 1930-, eds. The Magellanic Clouds: Proceedings of the 148th Symposium of the International Astronomical Union, held in Sydney, Australia, July 9-13, 1990. Dordrecht, The Netherlands: Kluwer, 1991.

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M, Braun Jochem, and Richtler Tom, eds. The magellanic clouds and other dwarf galaxies. Aachen: Shaker Verlag, 1998.

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1935-, Baschek B., Klare Gerhard, Lequeux James, and Sonderforschungsbereich 328, eds. New aspects of Magellanic cloud research: Proceedings of the Second European Meeting on the Magellanic Clouds. Berlin: Springer-Verlag, 1993.

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You-Hua, Chu, ed. New views of the Magellanic Clouds: Proceedings of the 190th Symposium of the International Astronomical Union held in Victoria, Canada, 12-17 July 1998. [San Francisco, Calif.]: Published on behalf of the International Astronomical Union by Astronomical Society of the Pacific, 1999.

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Observatory, Smithsonian Astrophysical, and United States. National Aeronautics and Space Administration., eds. ROSAT PSPC observations of CL0016+16: NASA grant NAG5-2156, annual report no. 4 for the period 15 December 1995 through 14 December 1996. Cambridge, Mass: Smithsonian Institution, Astrophysical Observatory, 1996.

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Schwering, P. B. W., and F. P. Israel. Atlas and Catalogue of Infrared Sources in the Magellanic Clouds. Dordrecht: Springer Netherlands, 1990. http://dx.doi.org/10.1007/978-94-009-0537-5.

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Schwering, P. B. W. Atlas and catalogue of infrared sources in the Magellanic Clouds. Dordrecht: Kluwer Academic Publishers, 1990.

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Book chapters on the topic "Magellanic Clouds"

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Mebold, Ulrich. "High Velocity Clouds Near the Magellanic Clouds." In The Magellanic Clouds, 463–68. Dordrecht: Springer Netherlands, 1991. http://dx.doi.org/10.1007/978-94-011-3432-3_123.

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Westerlund, B. E. "The Magellanic Clouds." In Astrophysics and Space Science Library, 305–14. Dordrecht: Springer Netherlands, 1994. http://dx.doi.org/10.1007/978-94-011-0794-5_31.

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Shuter, W. L. H. "The Magellanic Stream." In The Magellanic Clouds, 483–84. Dordrecht: Springer Netherlands, 1991. http://dx.doi.org/10.1007/978-94-011-3432-3_130.

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Feast, M. W. "The Magellanic Clouds: Distance, Structure, Chemical Composition." In The Magellanic Clouds, 1–5. Dordrecht: Springer Netherlands, 1991. http://dx.doi.org/10.1007/978-94-011-3432-3_1.

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Hodge, Paul. "Dust in the Magellanic Clouds." In The Magellanic Clouds, 57–62. Dordrecht: Springer Netherlands, 1991. http://dx.doi.org/10.1007/978-94-011-3432-3_10.

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Tobin, William, A. C. Gilmore, Alan Wadsworth, and S. R. D. West. "First CCD Observations of Magellanic Cloud Variable Stars from the Mt John University Observatory, New Zealand." In The Magellanic Clouds, 381. Dordrecht: Springer Netherlands, 1991. http://dx.doi.org/10.1007/978-94-011-3432-3_100.

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Humphreys, R. M., R. P. Kudritzki, and H. Groth. "The Anomalous A-Type Supergiants in the Magellanic Clouds — Evidence for Post-Red Supergiant Evolution." In The Magellanic Clouds, 382–83. Dordrecht: Springer Netherlands, 1991. http://dx.doi.org/10.1007/978-94-011-3432-3_101.

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Welch, Douglas L., Patrick Côté, Mario Mateo, and Barry F. Madore. "The Variable Star Population of NGC 1866." In The Magellanic Clouds, 384–85. Dordrecht: Springer Netherlands, 1991. http://dx.doi.org/10.1007/978-94-011-3432-3_102.

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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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Jüttner, A., O. Stahl, B. Wolf, and B. Baschek. "Element Abundances from B Stars in the Magellanic Clouds." In The Magellanic Clouds, 388–89. Dordrecht: Springer Netherlands, 1991. http://dx.doi.org/10.1007/978-94-011-3432-3_104.

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Conference papers on the topic "Magellanic Clouds"

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Blair, William P., Cristina M. Oliveira, Stephanie M. LaMassa, Serah Gutman, Charles W. Danforth, Alex W. Fullerton, Ravi Sankrit, et al. "The FUSE∕MAST Magellanic Clouds Legacy Project: A New Resource for Magellanic Clouds Researchers." 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/10.1063/1.3154082.

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Xue, Rui, and Tony Wong. "ROTATIONALLY EXCITED H2 IN THE MAGELLANIC CLOUDS." In 69th International Symposium on Molecular Spectroscopy. Urbana, Illinois: University of Illinois at Urbana-Champaign, 2014. http://dx.doi.org/10.15278/isms.2014.rf14.

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Hughes, John P. "Young supernova remnants in the Magellanic Clouds." In The eleventh astrophysics conference on young supernova remnants. AIP, 2001. http://dx.doi.org/10.1063/1.1377130.

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Meixner, Margaret, Eli Dwek, Tea Temim, Kirill Tschernyshyov, Martha Boyer, Christa Gall, and Rafael Eufrasio. "EvolutioN of Grains in the MAgellanic clouds (ENiGMA)." In The Life Cycle of Dust in the Universe: Observations, Theory, and Laboratory Experiments. Trieste, Italy: Sissa Medialab, 2014. http://dx.doi.org/10.22323/1.207.0017.

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van Loon, Jacco Th. "ASKAP and MeerKAT surveys of the Magellanic Clouds." In ISKAF2010 Science Meeting. Trieste, Italy: Sissa Medialab, 2010. http://dx.doi.org/10.22323/1.112.0085.

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Haberl, F. "The X-ray source populations of the magellanic clouds." In X-RAY ASTRONOMY: Stellar Endpoints,AGN, and the Diffuse X-ray Background. AIP, 2001. http://dx.doi.org/10.1063/1.1434659.

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Cornett, Robert H., Joan Hollis, and Theodore P. Stecher. "Comparison of UV and Hα morphologies in the Magellanic Clouds." In The ultraviolet universe at low and high redshift. AIP, 1997. http://dx.doi.org/10.1063/1.53779.

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Rajoelimanana, Andry, Pieter Meintjes, and Phil Charles. "Multi-Wavelength Properties of Be/XRay Binaries in the Magellanic Clouds." In 4th Annual Conference on High Energy Astrophysics in Southern Africa. Trieste, Italy: Sissa Medialab, 2017. http://dx.doi.org/10.22323/1.275.0036.

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Delmotte, Nausicaa, Daniel Egret, Cecile Loup, and Maria-Rosa Cioni. "Cross-matching DENIS and 2MASS point sources toward the Magellanic Clouds." In International Symposium on Optical Science and Technology, edited by Jean-Luc Starck and Fionn D. Murtagh. SPIE, 2001. http://dx.doi.org/10.1117/12.447187.

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STUCHLÍK, Z., and J. SCHEE. "INFLUENCE OF COSMOLOGICAL CONSTANT ON MAGELLANIC CLOUDS MOTION AND OTHER RELEVANT INFLUENCES." In Proceedings of the MG13 Meeting on General Relativity. WORLD SCIENTIFIC, 2015. http://dx.doi.org/10.1142/9789814623995_0055.

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Reports on the topic "Magellanic Clouds"

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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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The Magellan Final Report on Cloud Computing. Office of Scientific and Technical Information (OSTI), December 2011. http://dx.doi.org/10.2172/1076794.

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