scholarly journals HI Supergiant Shells in the Large Magellanic Cloud

1998 ◽  
Vol 15 (1) ◽  
pp. 132-135 ◽  
Author(s):  
S. Kim ◽  
L. Staveley-Smith ◽  
R. J. Sault ◽  
M. J. Kesteven ◽  
D. McConnell ◽  
...  
Keyword(s):  
Interstellar Medium ◽  
Complex Structure ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Camera Lens ◽  
Hi Shells

AbstractThe recently completed HI mosaic survey of the Large Magellanic Cloud (Kim et al. 1997) reveals complex structure in the interstellar medium, including filaments, arcs, holes and shells. We have catalogued giant and supergiant HI shells and searched for correlations with Hα emission, using a new image taken with a camera lens mounted on the 16-inch telescope at Siding Spring Observatory.

scholarly journals The interstellar medium of the Magellanic Clouds from absorption lines

1991 ◽  
Vol 148 ◽  
pp. 401-406 ◽  
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.

scholarly journals The Absorption Line Systems of the Supershell LMC2 in the Large Magellanic Cloud

1999 ◽  
Vol 190 ◽  
pp. 154-155
Author(s):  
Adeline Caulet
Keyword(s):  
Optical Absorption ◽  
Interstellar Medium ◽  
Gas Phase ◽  
Absorption Line ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Absorption Lines

The interstellar medium of LMC2, a well studied supershell in the Large Magellanic Cloud, has been probed in UV and optical absorption lines. The data allow to derive the kinematics, abundances and depletions of gas clouds in this supershell. The relative gas-phase abundances of observed elements with respect to sulphur are useful to determine the origins of the supershell absorption-line clouds.

scholarly journals IRAS Observations of Collisionally Heated Dust in Large Magellanic Cloud Supernova Remnants

1988 ◽  
Vol 101 ◽  
pp. 383-386
Author(s):  
James R. Graham ◽  
A. Evans ◽  
J.S. Albinson ◽  
M.F. Bode ◽  
W.P.S. Meikle
Keyword(s):  
Interstellar Medium ◽  
Supernova Remnants ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Substantial Fraction ◽  
X Ray ◽  
Ir Sources ◽  
Atomic Cooling ◽  
Dust Grain ◽  
Ir Emission

AbstractIRAS additional observations show that luminous (104−105 L⊙) far-IR sources are associated with the Large Magellanic Cloud (LMC) supernova remnants N63A, N49, N49B, and N186D. Comparison of the IRAS and X-ray data shows that a substantial fraction of the IR emission from three of the SNRs can be accounted for by collisionally heated dust. The ratio of dust-grain cooling to total atomic cooling is ~10 in X-ray emitting gas (T~106 K). We show why dust cooling does not dominate, but probably speeds SNR evolution in an inhomogeneous interstellar medium.

scholarly journals Supersoft X-ray nebulae in the Large Magellanic Cloud

2020 ◽  
Vol 497 (3) ◽  
pp. 3234-3250 ◽  
Author(s):  
Diego A Farias ◽  
Alejandro Clocchiatti ◽  
Tyrone E Woods ◽  
Armin Rest
Keyword(s):  
Interstellar Medium ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
The Other ◽  
X Rays ◽  
X Ray ◽  
Upper Limits ◽  
Type Ia ◽  
Source Models ◽  
Flux Measurements

ABSTRACT Supersoft X-rays sources (SSSs) have been proposed as potential Type Ia supernova (SN Ia) progenitors. If such objects are indeed persistently X-ray luminous and embedded in sufficiently dense interstellar medium (ISM), they will be surrounded by extended nebular emission. These nebulae should persist even long after an SN Ia explosion, due to the long recombination and cooling times involved. With this in mind, we searched for nebular [O iii] emission around four SSSs and three SNRs in the Large Magellanic Cloud, using the 6.5-m Baade telescope at Las Campanas Observatory and the imacs camera. We confirm that, out of the four SSS candidates, only CAL 83 can be associated with an [O iii] nebula. The [O iii] luminosity for the other objects is constrained to ≲17 per cent of that of CAL 83 at 6.8 pc from the central source. Models computed with the photoionization code cloudy indicate that either the ISM densities in the environments of CAL 87, RX J0550.0-7151, and RX J0513.9-6951 must be significantly lower than surrounding CAL 83 or the average X-ray luminosities of these sources over the last ≲10  000 yr must be significantly lower than presently observed, in order to be consistent with the observed luminosity upper limits. For the three SNRs we consider (all with ages <1000 yr), our [O iii] flux measurements together with the known surrounding ISM densities strongly constrain the ionizing luminosity of their progenitors in the last several thousand years, independent of the progenitor channel.

scholarly journals Stochastic Starformation and Bubbles in the Large Magellanic Cloud

1984 ◽  
Vol 108 ◽  
pp. 89-90
Author(s):  
J. V. Feitzinger
Keyword(s):  
Interstellar Medium ◽  
Radiation Pressure ◽  
Hii Regions ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Shell Structures ◽  
Stellar Winds ◽  
Bubble Structure ◽  
Ring Nebulae

Nearly all places in the LMC where ring nebulae or shell structures in the neutral or ionized interstellar medium are observed, an OB association and/or WR-stars can be located (Braunsfurth, Feitzinger, 1983). Several mechanisms have been propsoed to generate shell or bubble structures: stellar winds, supernovae explosions, evolving HII regions, sequential starformation, collapsing hydrogen clouds interacting with stellar winds and radiation pressure. Ordered motions resulting in a shell or bubble structure are the result of almost any point like energy injection into the interstellar medium. Therefore all the mechanisms result in similar morphological structures, thus similar shapes can have heterogeneous origins.

The detection of X-rays from the hot interstellar medium of the Large Magellanic Cloud

1991 ◽  
Vol 374 ◽  
pp. 475 ◽  
Author(s):  
Q. Wang ◽  
T. Hamilton ◽  
D. J. Helfand ◽  
X. Wu
Keyword(s):  
Interstellar Medium ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
X Rays

scholarly journals THE INFLUENCE OF SUPERNOVA REMNANTS ON THE INTERSTELLAR MEDIUM IN THE LARGE MAGELLANIC CLOUD SEEN AT 20-600 μm WAVELENGTHS

2015 ◽  
Vol 799 (1) ◽  
pp. 50 ◽  
Author(s):  
Maša Lakićević ◽  
Jacco Th. van Loon ◽  
Margaret Meixner ◽  
Karl Gordon ◽  
Caroline Bot ◽  
...  
Keyword(s):  
Interstellar Medium ◽  
Supernova Remnants ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud

scholarly journals Molecular hydrogen emission in the interstellar medium of the Large Magellanic Cloud

2014 ◽  
Vol 446 (3) ◽  
pp. 2490-2504 ◽  
Author(s):  
N. Naslim ◽  
F. Kemper ◽  
S. C. Madden ◽  
S. Hony ◽  
Y.- H. Chu ◽  
...  
Keyword(s):  
Interstellar Medium ◽  
Molecular Hydrogen ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Hydrogen Emission

scholarly journals SPITZERSURVEY OF THE LARGE MAGELLANIC CLOUD, SURVEYING THE AGENTS OF A GALAXY'S EVOLUTION (SAGE). IV. DUST PROPERTIES IN THE INTERSTELLAR MEDIUM

2008 ◽  
Vol 136 (3) ◽  
pp. 919-945 ◽  
Author(s):  
Jean-Philippe Bernard ◽  
William T. Reach ◽  
Deborah Paradis ◽  
Margaret Meixner ◽  
Roberta Paladini ◽  
...  
Keyword(s):  
Interstellar Medium ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud
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