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Journal articles on the topic 'Magellanic Clouds'

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Author: Grafiati

Published: 4 June 2021

Last updated: 8 June 2024

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1

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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2

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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3

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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4

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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5

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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6

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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7

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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8

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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9

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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10

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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11

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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12

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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13

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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14

Jeong, Yeuncheol, Alexander V. Yushchenko, Vira F. Gopka, Volodymyr O. Yushchenko, Valery V. Kovtyukh, and Svetlana V. Vasil’eva. "Magellanic Clouds Cepheids: Thorium Abundances." Journal of Astronomy and Space Sciences 35, no. 1 (March 2018): 19–30. http://dx.doi.org/10.5140/jass.2018.35.1.19.

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The analysis of the high-resolution spectra of 31 Magellanic Clouds Cepheid variables enabled the identification of thorium lines. The abundances of thorium were found with spectrum synthesis method. The calculated thorium abundances exhibit correlations with the abundances of other chemical elements and atmospheric parameters of the program stars. These correlations are similar for both Clouds. The correlations of iron abundances of thorium, europium, neodymium, and yttrium relative to the pulsational periods are different in the Large Magellanic Cloud (LMC) and the Small Magellanic Cloud (SMC), namely the correlations are negative for LMC and positive or close to zero for SMC. One of the possible explanations can be the higher activity of nucleosynthesis in SMC with respect to LMC in the recent several hundred million years.

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15

Westerlund, B. E. "The Kinematics of the Magellanic Clouds." Symposium - International Astronomical Union 166 (1995): 273–82. http://dx.doi.org/10.1017/s0074180900228180.

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It is essential for our understanding of the evolution of the Magellanic System, comprising the Large and the Small Magellanic Cloud, the Intercloud or Bridge region and the Magellanic Stream, to know its motions in the past. The Clouds have a common envelope of neutral hydrogen; this indicates that they have been bound to each others for a long time. The Magellanic System moves in the gravitational potential of our Galaxy; it is exposed to ram pressure through its movement in the galactic halo. Both effects ought to be noticeable in their present structure and kinematics. It is generally assumed, but not definitely proven, that the Clouds have been bound to our Galaxy for at least the last 7 Gyr. Most models assume that the Clouds lead the Magellanic Stream. The interaction between the Clouds has influenced their structure and kinematics severely. The effects should be possible to trace in the motions of their stellar and gaseous components as pronounced disturbances. Recent astrometric contributions in this field show a great promise for the future if still higher accuracy can be achieved.

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16

STUCHLÍK, ZDENĚK, and JAN SCHEE. "COMPARISON OF GENERAL RELATIVISTIC AND PSEUDO-NEWTONIAN DESCRIPTION OF MAGELLANIC-CLOUDS MOTION IN THE FIELD OF MILKY WAY." International Journal of Modern Physics D 21, no. 04 (April 2012): 1250031. http://dx.doi.org/10.1142/s0218271812500319.

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We test precision of the Cosmological Paczynski–Wiita (CPW) potential reflecting properties of the Schwarzschild–de Sitter (SdS) spacetimes in modeling dynamical phenomena related to galaxy motion. We consider a simplified model of Magellanic Clouds moving in the field of Milky Way as test particles. Time evolution of their position along trajectories obtained in the CPW framework using the notion of Newtonian time is compared to the one obtained in the fully general relativistic (GR) approach when the time evolution is expressed in terms of time related to the location of Earth in the Galaxy field. The differences in the position-evolution of the Magellanic Clouds obtained in the CPW and GR approaches are given for appropriately chosen values of the Milky Way mass. It is shown that the integrated relativistic corrections represent ~10-5 part of the Newtonian CPW predictions for the orbital characteristics of the motion and slightly grow with Galaxy mass growing, being at least by one order higher than the local scaling GR corrections. The integrated orbital GR corrections thus could be important only in very precise modeling of the motion of Magellanic Clouds. The CPW framework is used to show that, quite surprisingly, the influence of the cosmological constant on the Magellanic Clouds motion can be strong and significantly alters the trajectories of Magellanic Clouds and time evolution along them. The relative contribution of the cosmological constant is ~10-1 or higher. It is most profoundly demonstrated by the increase of the binding mass that represents 22% for Small Magellanic Cloud and even 47% for Large Magellanic Cloud, putting serious doubts on gravitational binding to the Milky Way in the later case.

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17

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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18

Johnston, S., A. Parthasarathy, R. A. Main, J. P. Ridley, B. S. Koribalski, M. Bailes, S. J. Buchner, et al. "The thousand-pulsar-array programme on MeerKAT VII: polarisation properties of pulsars in the Magellanic Clouds." Monthly Notices of the Royal Astronomical Society 509, no. 4 (November 23, 2021): 5209–17. http://dx.doi.org/10.1093/mnras/stab3360.

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ABSTRACT The Magellanic Clouds are the only external galaxies known to host radio pulsars. The dispersion and rotation measures of pulsars in the Clouds can aid in understanding their structure, and studies of the pulsars themselves can point to potential differences between them and their Galactic counterparts. We use the high sensitivity of the MeerKAT telescope to observe 17 pulsars in the Small and Large Magellanic Clouds in addition to five foreground (Galactic) pulsars. We provide polarisation profiles for 18 of these pulsars, improved measurements of their dispersion and rotation measures, and derive the mean parallel magnetic field along the lines of sight. The results are broadly in agreement with expectations for the structure and strength of the magnetic field in the Large and Small Magellanic Clouds. The Magellanic Cloud pulsars have profiles which are narrower than expected from the period-width relationship and we show this is due to selection effects in pulsar surveys rather than any intrinsic difference between the population of Galactic and Magellanic objects.

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19

Caldwell, John A. R., and C. David Laney. "Cepheids in the Magellanic Clouds." Symposium - International Astronomical Union 148 (1991): 249–57. http://dx.doi.org/10.1017/s0074180900200545.

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Cepheid variables provide a key to understanding the structure and distance of the Magellanic Clouds, as well as providing accurate reddenings there. Recent major observing programs have continually expanded the data base of photometry and velocities. It is important to try to reconcile the plethora of Cepheid data into a consonant picture of the three-dimensional spatial structure of the Clouds and to compare in a consistent manner the bulk Cloud distance moduli found by several photometric methods.

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20

Westerlund, B. E. "An overview of the structure and kinematics of the Magellanic Clouds." Symposium - International Astronomical Union 148 (1991): 15–23. http://dx.doi.org/10.1017/s0074180900199942.

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A vast amount of observational data concerning the structure and kinematics of the Magellanic Clouds is now available. Many basic quantities (e.g. distances and geometry) are, however, not yet sufficiently well determined. Interactions between the Small Magellanic Cloud (SMC), the Large Magellanic Cloud (LMC) and our Galaxy have dominated the evolution of the Clouds, causing bursts of star formation which, together with stochastic self-propagating star formation, produced the observed structures. In the youngest generation in the LMC it is seen as an intricate pattern imitating a fragmented spiral structure. In the SMC much of the fragmentation is along the line of sight complicating the reconstruction of its history. The violent events in the past are also recognizable in complex velocity patterns which make the analysis of the kinematics of the Clouds difficult.

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Hatzidimitriou, D. "The Study of Stellar Populations and Dynamics in the Small Magellanic Cloud using the UKST." International Astronomical Union Colloquium 148 (1995): 396–404. http://dx.doi.org/10.1017/s0252921100022260.

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AbstractThe combination of the wide field of Schmidt telescope photographic plates with fast measuring machines such as COSMOS and APM, had a major impact on the study of the global properties of the Magellanic Clouds. Results (based on UKST data) regarding the stellar populations and dynamics of the Small Magellanic Cloud are described here in some detail. The stellar content and kinematics of the intercloud region are also outlined, with particular emphasis on the importance of this region in understanding the interaction between the Magellanic Clouds.

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22

Gatto, M., V. Ripepi, M. Bellazzini, M. Cignoni, M.-R. L. Cioni, M. Dall’Ora, G. Longo, M. Marconi, P. Schipani, and M. Tosi. "A search for star clusters in the outskirts of the Large Magellanic Cloud: indication of clusters in the age gap." Monthly Notices of the Royal Astronomical Society 499, no. 3 (September 30, 2020): 4114–39. http://dx.doi.org/10.1093/mnras/staa3003.

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ABSTRACT The YMCA (Yes, Magellanic Clouds Again) and STEP (The SMC in Time: Evolution of a Prototype interacting late-type dwarf galaxy) projects are deep g, i photometric surveys carried out with the VLT Survey Telescope (VST) and devoted to study the outskirts of the Magellanic System. A main goal of YMCA and STEP is to identify candidate stellar clusters and complete their census out to the outermost regions of the Magellanic Clouds. We adopted a specific overdensity search technique coupled with a visual inspection of the colour–magnitude diagrams to select the best candidates and estimate their ages. To date, we analysed a region of 23 square degrees in the outskirts of the Large Magellanic Cloud, detecting 85 candidate cluster candidates, 16 of which have estimated ages falling in the so-called age gap. We use these objects together with literature data to gain insight into the formation and interaction history of the Magellanic Clouds.

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Bekki, Kenji. "Triggered star formation in the Magellanic Clouds." Proceedings of the International Astronomical Union 2, S237 (August 2006): 373–77. http://dx.doi.org/10.1017/s1743921307001755.

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AbstractWe discuss how tidal interaction between the Large Magellanic Cloud (LMC), the Small Magellanic Cloud (SMC), and the Galaxy triggers galaxy-wide star formation in the Clouds for the last ~0.2 Gyr based on our chemodynamical simulations on the Clouds. Our simulations demonstrate that the tidal interaction induces the formation of asymmetric spiral arms with high gas densities and consequently triggers star formation within the arms in the LMC. Star formation rate in the present LMC is significantly enhanced just above the eastern edge of the LMC's stellar bar owing to the tidal interaction. The location of the enhanced star formation is very similar to the observed location of 30 Doradus, which suggests that the formation of 30 Doradus is closely associated with the last Magellanic collision about 0.2 Gyr ago. The tidal interaction can dramatically compress gas initially within the outer part of the SMC so that new stars can be formed from the gas to become intergalactic young stars in the inter-Cloud region (e.g., the Magellanic Bridge). The metallicity distribution function of the newly formed stars in the Magellanic Bridge has a peak of [Fe/H] ~−0.8, which is significantly lower than the stellar metallicity of the SMC.

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Johansson, Lars E. B., Arto Heikkilä, and Hans Olofsson. "Molecular Line Observations in the Magellanic Clouds." Symposium - International Astronomical Union 190 (1999): 116–17. http://dx.doi.org/10.1017/s0074180900117553.

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We have observed spectral line emission from a sample of clouds in the Magellanic Clouds to investigate the effects of metallicity and FUV radiation on the physical and chemical properties of the interstellar medium. The clouds were identified by CO surveys and selected to cover a wide range of environments. We present molecular line data for five clouds in the LMC and one cloud in the SMC.

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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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Stanghellini, Letizia. "The population of Magellanic Cloud planetary nebulae." Proceedings of the International Astronomical Union 4, S256 (July 2008): 421–30. http://dx.doi.org/10.1017/s1743921308028810.

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AbstractIn this review we address the progress that has been made toward the understanding of Magellanic Cloud planetary nebulae (PNe) and their evolution since the last Magellanic Cloud Symposium. Planetary nebulae in the Magellanic Clouds are the key probes of stellar and circumstellar evolution, both for their known distances and relative vicinity, and for their broad metallicity range A selection of recent results is presented, including the HST study of PNe and their central stars, the study of the population of Magellanic Cloud PNe based on abundance analysis, the recent Spitzer analysis of their dust contents, and the use of Magellanic Cloud PNe to constrain the distance scale of Galactic PNe.

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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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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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29

Booth, R. S., and Th De Graauw. "Molecules in the Magellanic Clouds." Symposium - International Astronomical Union 148 (1991): 415–20. http://dx.doi.org/10.1017/s0074180900201046.

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In this short review we describe recent new observations of millimetre transitions of molecules in selected regions of the Magellanic Clouds. The observations were made using the Swedish-ESO Submillimetre Telescope, SEST, (Booth et al. 1989), the relatively high resolution of which facilitates, for the first time, observations of individual giant molecular clouds in the Magellanic Clouds. We have mapped the distribution of the emission from the two lowest rotational transitions of 12CO and 13CO and hence have derived excitation conditions for the molecule. In addition, we have observed several well-known interstellar molecules in the same regions, thus doubling the number of known molecules in the Large Magellanic Cloud (LMC). The fact that all the observations have been made under controlled conditions with the same telescope enables a reasonable intercomparison of the molecular column densities. In particular, we are able to observe the relative abundances among the different isotopically substituted species of CO.

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30

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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31

Mcconnell, D., P. M. Mcculloch, P. A. Hamilton, J. G. Ables, P. J. Hall, C. E. Jacka, and A. J. Hunt. "Radio pulsars in the Magellanic Clouds." Symposium - International Astronomical Union 148 (1991): 322. http://dx.doi.org/10.1017/s0074180900200661.

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The Large Magellanic Cloud (LMC) and Small Magellanic Cloud (SMC) have been searched for radio pulsars using the 64-m Parkes radiotelescope. The search has resulted in the discovery of four pulsars. Observed dispersion measures to each suggest that three lie in the Clouds (two in the LMC, one in the SMC) and that the fourth, which was found in the direction of the LMC, is a foreground object belonging to the galactic pulsar population.

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32

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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33

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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34

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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35

Harris, Jason, Dennis Zaritsky, Eva K. Grebel, and Ian Thompson. "The Star Formation History of the Magellanic Clouds: A Preliminary Report." Symposium - International Astronomical Union 190 (1999): 347–48. http://dx.doi.org/10.1017/s0074180900118182.

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We present a method to determine the star formation history (SFH) of a mixed stellar population, based on an iterative maximum Likelihood comparison of stellar photometry to model color-magnitude diagrams. We demonstrate the algorithm on a subregion of the Large Magellanic Cloud, observed as part of our ongoing Magellanic Clouds Photometric Survey. We will eventually perform this analysis on hundreds of regions in both Clouds, resulting in a homogeneous SFH map of these galaxies.

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36

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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37

Reid, Neill, and J. R. Mould. "Asymptotic Giant Branch Stars in the Magellanic Clouds." Symposium - International Astronomical Union 148 (1991): 363–64. http://dx.doi.org/10.1017/s0074180900200855.

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Since the pioneering objective prism surveys by Westerlund (1960) and Blanco et al. (1980), the Magellanic Clouds have proved a fruitful site for exploring the evolution of AGB stars. We have used photometric techniques to extend the prism C-star surveys to M- and S-type AGB stars, constructing luminosity functions and obtaining spectra of individual stars for comparison with theoretical predictions. We have concentrated on the Large Magellanic Cloud (LMC), but we have recently obtained observations of luminous red giants in a region of the Small Magellanic Cloud (SMC). In this paper we compare the results from these studies of the two satellite systems.

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38

Dempsey, J., N. M. McClure-Griffiths, K. Jameson, and F. Buckland-Willis. "Cold H i ejected into the Magellanic Stream." Monthly Notices of the Royal Astronomical Society 496, no. 1 (June 8, 2020): 913–20. http://dx.doi.org/10.1093/mnras/staa1602.

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ABSTRACT We report the direct detection of cold H i gas in a cloud ejected from the Small Magellanic Cloud (SMC) towards the Magellanic Stream. The cloud is part of a fragmented shell of H i gas on the outskirts of the SMC. This is the second direct detection of cold H i associated with the Magellanic Stream using absorption. The cold gas was detected using 21-cm H i absorption-line observations with the Australia Telescope Compact Array (ATCA) towards the extra-galactic source PMN J0029−7228. We find a spin (excitation) temperature for the gas of 68 ± 20 K. We suggest that breaking super shells from the Magellanic Clouds may be a source of cold gas to supply the rest of the Magellanic Stream.

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39

Lucchini, Scott, Elena D’Onghia, and Andrew J. Fox. "Properties of the Magellanic Corona." Astrophysical Journal 967, no. 1 (May 1, 2024): 16. http://dx.doi.org/10.3847/1538-4357/ad3c3b.

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Abstract We characterize the Magellanic Corona, the warm gaseous halo around the Large Magellanic Cloud (LMC). The Corona is a key ingredient in the formation of the Magellanic Stream and has recently been observed in high-ion absorption around the LMC. In this work, we present a suite of high-resolution hydrodynamical simulations to constrain its total mass and temperature prior to the infall of the Magellanic Clouds to our Galaxy. We find that the LMC is able to host a stable Corona before and during its approach to the MW through to the present day. With a Magellanic Corona of >2 × 109 M ⊙ at 3 × 105 K, our simulations can reproduce the observed total mass of the neutral and ionized components of the Trailing Stream, the size of the LMC disk, the ionization fractions along the Stream, the morphology of the neutral gas, and the on-sky extent of the ionized gas. The Corona plays an integral role in the survival, morphology, and composition of the Magellanic Clouds and the Trailing Stream.

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40

Putman, M. E. "The Magellanic System's Interactive Formations." Publications of the Astronomical Society of Australia 17, no. 1 (2000): 1–5. http://dx.doi.org/10.1071/as00001.

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AbstractThe interaction between the Galaxy and the Magellanic Clouds has resulted in several high-velocity complexes which are connected to the Clouds. The complexes are known as the Magellanic Bridge, an HI connection between the Large and Small Magellanic Clouds, the Magellanic Stream, a 10° × 100° HI filament which trails the Clouds, and the Leading Arm, a diffuse HI filament which leads the Clouds. The mechanism responsible for these features formation remains under some debate, with the lack of detailed HI observations being one of the limiting factors in resolving the issue. Here I present several large mosaics of HI Parkes All-Sky Survey (HIPASS) data which show the full extent of the three Magellanic complexes at almost twice the resolution of previous observations. These interactive features are connected, but unique in their spatial and velocity distribution. The differences may shed light on their origin and present environment. Dense clumps of HI along the sightline to the Sculptor Group, which may or may not be associated with the Magellanic complexes, are also discussed.

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41

Udalski, A. "New results on OGLE Cepheids and PL relations in the LMC and SMC." International Astronomical Union Colloquium 193 (2004): 75–82. http://dx.doi.org/10.1017/s025292110001037x.

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AbstractWe present results of the search for pulsating variable stars in the Magellanic Cloud fields covering central parts of these galaxies. The data were collected during the second phase of the Optical Gravitational Lensing Experiment survey (OGLE-II) from 1997 to 2000. In total, several thousand pulsating stars (Cepheids, RR Lyr) were found in both Magellanic Clouds. The photometric data of all objects are available to the astronomical community from the OGLE Internet archive. We present basic properties of pulsating stars in the Magellanic Clouds including Period–Luminosity relations for Cepheids. We also discuss observational prospects for the pulsating star field in the ongoing third phase of the OGLE project (OGLE-III) which started in 2001.

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42

Wood, P. R., M. S. Bessell, and J. B. Whiteoak. "Detection of the first extra-galactic OH/IR star." Symposium - International Astronomical Union 122 (1987): 241. http://dx.doi.org/10.1017/s0074180900156505.

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A search has been made for 1612 MHz OH maser emission from OH/IR stars in the Magellanic Clouds. Candidate objects were selected mainly on the basis of their 25μm flux densities and the 25 to 12μm flux ratio as given in the IRAS point source catalog; two known long-period variables and two HII regions (30 Doradus and N159) were also examined. One OH source (IRAS 04553-6825) was detected, this being the first OH/IR star found in the Magellanic Clouds. Upper limits were placed on the flux for 17 other sources. The expansion velocity of the circumstellar material surrounding IRAS 04553-6825, as indicated by the OH peak separation of 11 km s−1, is surprisingly small compared to Galactic sources of similar bolometric and OH luminosity. The OH intensity of IRAS 04553-6825, and the upper flux limits placed on many of the other objects examined, indicate that Magellanic Cloud OH/IR stars do not emit OH as strongly as their Galactic counterparts of similar 25μm/12μm flux ratio. Both the low expansion velocity of IRAS 04553-6825 and the low OH intensity of the Magellanic Cloud infrared sources may be explained by the low metal abundance in the Clouds.

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43

Shull, Peter, John Dyson, and Franz Kahn. "A Model of SNR Evolution for an O-Star in a Cloudy ISM." International Astronomical Union Colloquium 101 (1988): 231–34. http://dx.doi.org/10.1017/s0252921100102416.

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AbstractWe present an analytical model of SNR evolution in a cloudy interstellar medium for a single progenitor star of spectral type 05 V. The model begins with the progenitor on the zero-age main sequence, includes the effects of the star’s wind and ionizing photons, and ends with the SNR’s assimilation by the ISM. We assume that the ISM consists of atomic clouds, molecular clouds, and a hot intercloud phase. The type of SNR that results bears a strong resemblance to N63A in the Large Magellanic Cloud.

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44

Bekki, Kenji, and Masashi Chiba. "Dynamical Influences of the Last Magellanic Interaction on the Magellanic Clouds." Publications of the Astronomical Society of Australia 24, no. 1 (2007): 21–29. http://dx.doi.org/10.1071/as06023.

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AbstractWe investigate the present distributions of gas and young stars in the Large and Small Magellanic Clouds (LMC and SMC) based on fully self-consistent numerical simulations of the Clouds for the last ∼0.8 Gyr. Our principal results, which can be tested against observations, are as follows. The last dynamical and hydrodynamical interaction between the Clouds about ∼0.2 Gyr ago can form the apparently off-center bar and peculiar Hı spirals of the LMC. The present spatial distributions of young stars with ages less than ∼20 Myr in the LMC can be significantly asymmetric and clumpy owing to the interaction. A small but non-negligible fraction of stellar and gaseous components can be transferred from the SMC into the LMC during the interaction to form diffuse halo components around the LMC. The burst of star formation in the SMC can be synchronized with that of the LMC about 0.2 Gyr ago in some models. New stars can form from gas in the SMC's tidal tails, one of which can be observed as the Magellanic Bridge (MB). The metallicity distribution function of new stars in the MB has a peak of [Fe/H] ∼ −0.8, which is significantly smaller than the stellar metallicity of the SMC. Based on these results, we discuss the origin of 30 Doradus, the southern molecular ridge of the LMC, the globular cluster ESO 121-SC03, metal-poor inter-Cloud stars within the MB, and giant Hı holes of the LMC.

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45

Garnett, Donald R. "Element Abundances in Magellanic Cloud H II Regions from Carbon to Argon." Symposium - International Astronomical Union 190 (1999): 266–72. http://dx.doi.org/10.1017/s0074180900118017.

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I review measurements of heavy element abundances within H II regions in the Magellanic Clouds, highlighting in particular improved determinations of carbon abundances based on UV spectroscopy with Hubble Space Telescope. In general, the Magellanic Cloud H II regions show average underabundances in O, Ne, and S (relative to their Galactic counterparts) that are similar to those measured in Magellanic Cloud stars. However, comparison of stars and ionized gas shows discrepancies in C and N abundances that may be related to recently recognized mixing processes that may be operating in massive stars.

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46

Mebold, Ulrich. "High velocity clouds near the Magellanic Clouds." Symposium - International Astronomical Union 148 (1991): 463–68. http://dx.doi.org/10.1017/s0074180900201162.

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High velocity clouds (HVCs) of neutral atomic hydrogen close to the position of the Magellanic Clouds (MCs) and the Magellanic Stream (Stream) are reviewed. The gas observed at velocities of +70 km/s and +130 km/s in front of the LMC is probably associated with ordinary HVCs in the galactic halo. This is not the case for the gas observed between +150 and +170 km/s which is more likely associated with the MCs. The HVCs observed superimposed onto the Stream are possibly remnants of collisions between a gaseous polar ring around our Galaxy and the bridge region between the MCs. The HVCs found close to and “behind” the tip of the Stream may be regarded as shreds of the Stream precipitating toward the galactic disk. The chemical composition, the radiation field and the temperature in the Stream is discussed in the context of the first spin temperature determination by Wakker (1990), of an HVC.

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47

Rubio, Mónica. "Giant Molecular Clouds and Cluster Formation." Symposium - International Astronomical Union 207 (2002): 499–504. http://dx.doi.org/10.1017/s0074180900224303.

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We will review the present knowledge of molecular cloud properties and its relation to star formation. We will discuss the evidence for cluster formation associated with giant molecular clouds, and will concentrate on recent results in our Galaxy and the Magellanic Clouds.

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48

Ohno, Takahiro, Kazuki Tokuda, Ayu Konishi, Takeru Matsumoto, Marta Sewiło, Hiroshi Kondo, Hidetoshi Sano, et al. "An Unbiased CO Survey Toward the Northern Region of the Small Magellanic Cloud with the Atacama Compact Array. II. CO Cloud Catalog." Astrophysical Journal 949, no. 2 (May 31, 2023): 63. http://dx.doi.org/10.3847/1538-4357/accadb.

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Abstract The nature of molecular clouds and their statistical behavior in subsolar metallicity environments are not fully explored yet. We analyzed data from an unbiased CO (J = 2–1) survey at the spatial resolution of ∼2 pc in the northern region of the Small Magellanic Cloud with the Atacama Compact Array to characterize the CO cloud properties. A cloud-decomposition analysis identified 426 spatially/velocity-independent CO clouds and their substructures. Based on the cross-matching with known infrared catalogs by Spitzer and Herschel, more than 90% CO clouds show spatial correlations with point sources. We investigated the basic properties of the CO clouds and found that the radius–velocity linewidth (R–σ v ) relation follows the Milky Way-like power-law exponent, but the intercept is ∼1.5 times lower than that in the Milky Way. The mass functions (dN/dM) of the CO luminosity and virial mass are characterized by an exponent of ∼1.7, which is consistent with previously reported values in the Large Magellanic Cloud and in the Milky Way.

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49

Wayte, S. R. "The interacting Magellanic System." Symposium - International Astronomical Union 148 (1991): 447–52. http://dx.doi.org/10.1017/s0074180900201149.

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The Magellanic System is viewed focusing on the global interactions in the System. These give insight into its history and structure. The past orbits of the Magellanic Clouds (MCs) are examined. A tidal encounter between the Large and Small Magellanic Clouds (LMC, SMC) has almost certainly occurred within the last 109 yrs. This hypothesis is supported by the observed structure of the Magellanic System, and so is accepted. The Magellanic Stream is an indirect result of the tidal encounter which is crucial to understanding the Magellanic System. It is a complex interacting gas feature, bifurcated along its entire length with many anomalous velocity H I clouds alongside. The possible models for the Magellanic Stream are examined and here I propose that its origin is due to the collision of a multi-phase halo with the vast region of gas between the LMC and the SMC. In this respect the polar subsystem around our Galaxy is seen to be particularly important. The popular tidal model for the origin of the Magellanic Stream fails to satisfy key observational features, and is thus rejected.

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50

Boulanger, François. "Dust in the Magellanic Clouds." Proceedings of the International Astronomical Union 4, S256 (July 2008): 137–47. http://dx.doi.org/10.1017/s1743921308028378.

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AbstractThe Magellanic Clouds are important templates for studying the role interstellar dust plays as actor and tracer of galaxy evolution. Due to their proximity, the Large and Small Magellanic clouds are uniquely suited to put detailed Galactic dust studies in a global context. With a metal abundance lower than that of the Sun, the Magellanic Clouds also permit to characterize interstellar matter composition and structure as a function of metallicity. The presentation of spectacular results from the AKARI and Spitzer surveys was one of the highlights of this Magellanic Clouds meeting. This paper puts these results in context. I discuss UV extinction and IR emission signatures of carbon and silicate dust. I present diverse evidence of dust processing in the ISM. I illustrate the correlation between the mm emission of dust, and gas column density using Milky Way surveys. I conclude with three main results. Dust in the SMC is not carbon poor. The composition of interstellar dust reflects its processing in interstellar space and thereby depends on local conditions and its past history. In the Magellanic Clouds, far-IR and sub-mm observations are indicating that there may be significantly more cold interstellar matter, cold H i and H2 gas, than estimated from H i and CO observations.

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