Search for binary central stars of the Magellanic Clouds PNe

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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The interstellar medium of the Magellanic Clouds from absorption lines

Symposium - International Astronomical Union ◽

10.1017/s0074180900201022 ◽

1991 ◽

Vol 148 ◽

pp. 401-406 ◽

Cited By ~ 2

Author(s):

Klaas S. De Boer

Keyword(s):

Interstellar Medium ◽

Absorption Line ◽

Milky Way ◽

Large Magellanic Cloud ◽

Magellanic Cloud ◽

Magellanic Clouds ◽

Absorption Lines ◽

Small Magellanic Cloud ◽

General Aspects

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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Star clusters in the Magellanic Clouds

Symposium - International Astronomical Union ◽

10.1017/s0074180900200259 ◽

1991 ◽

Vol 148 ◽

pp. 161-164 ◽

Cited By ~ 1

Author(s):

S. van den Bergh

Keyword(s):

Cluster Formation ◽

Star Clusters ◽

Large Magellanic Cloud ◽

Magellanic Cloud ◽

Magellanic Clouds ◽

Open Clusters ◽

Small Magellanic Cloud ◽

Cloud Clusters ◽

The Galaxy

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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Spectroscopy of Overluminous Cepheids in the Magellanic Clouds

Symposium - International Astronomical Union ◽

10.1017/s0074180900040225 ◽

1984 ◽

Vol 108 ◽

pp. 223-224

Author(s):

Horace A. Smith ◽

Leo Connolly

Keyword(s):

Globular Cluster ◽

Large Magellanic Cloud ◽

Variable Stars ◽

Magellanic Cloud ◽

Magellanic Clouds ◽

Small Magellanic Cloud ◽

Single Star ◽

Rr Lyrae ◽

Short Period ◽

The Galaxy

The Small Magellanic Cloud is known to contain types of short period Cepheid variable stars not yet discovered in either the Large Magellanic Cloud or, with the exception of a single star, in the Galaxy. These variables can be divided into two categories: anomalous Cepheids and Wesselink-Shuttleworth (WS) stars. The former, which have also been found in dwarf spheroidal systems and in the globular cluster NGC 5466, have periods of 0.4–3 days, but average 0.7–1.0 mag. brighter than RR Lyrae and BL Her stars of equal period. The stars we call WS stars have periods less than about 1.1 day and, at MV = −1 to −2, are brighter than anomalous Cepheids of equal period.

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Ring Nebulae Associated with Wolf-Rayet Stars

Symposium - International Astronomical Union ◽

10.1017/s0074180900029235 ◽

1982 ◽

Vol 99 ◽

pp. 469-472

Author(s):

Y.-H. Chu

Keyword(s):

Selection Criteria ◽

Large Magellanic Cloud ◽

Magellanic Cloud ◽

Magellanic Clouds ◽

Small Magellanic Cloud ◽

The Galaxy ◽

Ring Nebulae ◽

Strict Selection

Using strict selection criteria, we have searched for ring nebulae associated with Wolf-Rayet stars in the Galaxy and the Magellanic Clouds. In our search, 15 WR ring nebulae are identified in the Galaxy (Chu 1981a; Chu 1981b, Paper G1), 9 in the Large Magellanic Cloud, and none in the Small Magellanic Cloud (Chu and Lasker 1980, Paper LI; Chu 1981a). We have subsequently observed the morphology and kinematics of these 24 nebulae to study their nature. The data and analyses are reported in G (galactic) and L (LMC) series of papers. These nebulae and their references are listed in Table 1. This table is nearly, but not quite, complete. An extremely careful search might result in more cases, e.g., NGC6357 (Lortet et al. 1981). In a later search by Heckathorn et al. (1982), more ring nebulae are suggested; however, only three cases (associated with HD92740, HD187282, and HD211564) are more convincing. We have obtained some data for these nebulae and will discuss them in a conclusion paper of the galactic series (Chu et al. 1982, Paper G8).

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Characterising the Protostellar Population of the Magellanic Clouds with VLT/SINFONI

Proceedings of the International Astronomical Union ◽

10.1017/s1743921316008449 ◽

2015 ◽

Vol 11 (S315) ◽

Author(s):

Jacob Ward ◽

Joana Oliveira ◽

Jacco van Loon ◽

Marta Sewilo

Keyword(s):

Star Formation ◽

Milky Way ◽

Large Magellanic Cloud ◽

Magellanic Cloud ◽

Magellanic Clouds ◽

Emission Lines ◽

Young Stellar Objects ◽

Small Magellanic Cloud ◽

Stellar Objects ◽

Accretion Rates

AbstractAt distances of ~50 kpc and ~60 kpc for the Large Magellanic Cloud (LMC) and Small Magellanic Cloud (SMC) respectively the Magellanic Clouds present us with a unique opportunity to study star formation in environments outside our own galaxy. Through Spitzer and Herschel photometry and spectroscopy, samples of Young Stellar Objects (YSOs) have been selected and spectroscpically confirmed in the Magellanic Clouds. Here we present some of the key results of our SINFONI K-band observations towards massive YSOs in the Magellanic Clouds. We resolve a number of Spitzer sources into multiple, previously unresolved, components and our analysis of emission lines suggest higher accretion rates and different disc properties compared with massive YSOs in the Milky Way.

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Interstellar gas around WO stars in the Galaxy and the Magellanic Clouds

Symposium - International Astronomical Union ◽

10.1017/s0074180900201113 ◽

1991 ◽

Vol 148 ◽

pp. 438-439

Author(s):

Tatiana A. Lozinskaya

Keyword(s):

Massive Stars ◽

Large Magellanic Cloud ◽

Magellanic Cloud ◽

Magellanic Clouds ◽

Stellar Winds ◽

Small Magellanic Cloud ◽

Interstellar Gas ◽

The Galaxy

The four oxygen-sequence WR stars, Sand 1 in the Small Magellanic Cloud (SMC), Sand 2 in the Large Magellanic Cloud (LMC), and WR 102 and WR 142 in the Galaxy represent the latest stage of the evolution of massive stars (Sanduleak 1971, Barlow and Hummer 1982, Moffatet al.1985). We have shown WR 102 to be a stripped CO core of a supermassive star (Dopitaet al.1990), probably seen only several thousand years before a SN explosion. The four stars are characterized by extremely energetic stellar winds –Vw from 4500 to 7400 km/s (Barlow and Hummer 1982, Dopitaet al.1990, Torreset al.1986). Examination of the environments of WO stars leads to the conclusion that the four objects appear to be associated with optical and/or IR shell-like structures, although the short WO-superwind does not prevail in the shell's formation.

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Planetary nebulae in the Magellanic Clouds and Local Group galaxies

Proceedings of the International Astronomical Union ◽

10.1017/s1743921312011003 ◽

2011 ◽

Vol 7 (S283) ◽

pp. 227-234

Author(s):

Warren A. Reid

Keyword(s):

Milky Way ◽

Local Group ◽

Large Magellanic Cloud ◽

Magellanic Cloud ◽

Magellanic Clouds ◽

The Past ◽

Spatially Resolved ◽

Multi Wavelength ◽

Large Telescopes ◽

Central Stars

AbstractThe Magellanic Clouds are close enough to the Milky Way to provide an excellent environment in which to study extragalactic PNe. Most of these PNe are bright enough to be spectroscopically observed and spatially resolved. With the latest high resolution detectors on today's large telescopes it is even possible to directly observe a large number of central stars. Magellanic Cloud (MC) PNe provide several astrophysical benefits including low overall extinction and a good sample size covering a large range of dynamic evolutionary timescales while the known distances provide a direct estimation of luminosity and physical dimensions. Multi-wavelength surveys are revealing intriguing differences between MC and Galactic PNe.Over the past 5 years there has been a substantial increase in the number of PNe discovered in the Large Magellanic Cloud (LMC) in particular. Deep surveys have allowed the faint end of the luminosity function to be investigated, finally providing a strong clue to its overall shape. In so doing, the surveys are approaching completeness, estimated at ~80% in the LMC (~120 deg2) and ~65% in the Small Magellanic Cloud (SMC) (~20 deg2).The number of galaxies comprising the Local Group (LG) and its outskirts has been growing steadily over the past 5 years and now numbers 48. Most of the 7 newly discovered galaxies are dwarf spheroidal (dSph) in structure and range from 7.6 to 755 kpc from the Milky Way. Nonetheless, there are no published searches for PNe in any of these galaxies to date. Apart from the LMC and Milky Way, the number of PN discoveries has been very modest and only one additional LG galaxy has been surveyed for PNe over the past 5 years. This paper provides the number of Local Group PNe currently known and estimates each galaxy's total PN population.

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An overview of the structure and kinematics of the Magellanic Clouds

Symposium - International Astronomical Union ◽

10.1017/s0074180900199942 ◽

1991 ◽

Vol 148 ◽

pp. 15-23 ◽

Cited By ~ 2

Author(s):

B. E. Westerlund

Keyword(s):

Star Formation ◽

Observational Data ◽

Spiral Structure ◽

Large Magellanic Cloud ◽

Magellanic Cloud ◽

Magellanic Clouds ◽

Line Of Sight ◽

Small Magellanic Cloud ◽

Complex Velocity ◽

The Past

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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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 ◽

10.1071/as98128 ◽

1998 ◽

Vol 15 (1) ◽

pp. 128-131 ◽

Cited By ~ 2

Author(s):

Miroslav D. Filipović ◽

Paul A. Jones ◽

Graeme L. White ◽

Raymond F. Haynes

Keyword(s):

Supernova Remnants ◽

Hii Regions ◽

Large Magellanic Cloud ◽

Magellanic Cloud ◽

Magellanic Clouds ◽

Small Magellanic Cloud

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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