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An Australia Telescope Compact Array 20-cm radio continuum study of the Large Magellanic Cloud
Hughes, A.,Staveley-Smith, L.,Kim, S.,Wolleben, M.,Filipović,, M. Blackwell Publishing Ltd 2007 MONTHLY NOTICES- ROYAL ASTRONOMICAL SOCIETY Vol.382 No.2
<P>ABSTRACT</P><P>We present a mosaic image of the 1.4-GHz radio continuum emission from the Large Magellanic Cloud (LMC) observed with the Australia Telescope Compact Array (ATCA) and the Parkes Telescope. The mosaic covers <IMG SRC='http://onlinelibrary.wiley.com/store/10.1111/j.1365-2966.2007.12466.x/asset/equation/MNR_12466_mu1.gif?v=1&s=3c55d39c3da8b7009e1ce58371b88f172bd55796'/> with an angular resolution of 40 arcsec, corresponding to a spatial scale of ∼10 pc in the LMC. The final image is suitable for studying emission on all scales between 40 arcsec and the surveyed area. In this paper, we discuss (i) the characteristics of the LMC's diffuse and compact radio continuum emission, (ii) the fraction of the emission produced by thermal processes and the implied star formation rate in the LMC and (iii) variations in the radio spectral index across the LMC. Two non-standard reduction techniques that we used to process the ATCA visibility data may be of interest for future wide-field radio continuum surveys. The data are open to the astronomical community and should be a rich resource for studies of individual objects such as supernova remnants, H <SMALL>II</SMALL> regions and planetary nebulae as well as extended features such as the diffuse emission from synchrotron radiation.</P>
A STUDY OF A TIDALLY INTERACTING BCD PAIR: ESO 435-IG20 AND ESO435-IG16
KIM, JINHYUB,SUNG, EON-CHANG,CHUNG, AEREE,STAVELEY-SMITH, LISTER The Korean Astronomical Society 2015 天文學論叢 Vol.30 No.2
We investigate $H\small{I}$ data for a pair of blue compact dwarf galaxies (BCDs), ESO 435-IG20 and ESO 435-IG16, obtained with the Australia Telescope Compact Array. The outer $H\small{I}$ disk is highly disturbed and asymmetric in both galaxies showing a gas tail and/or a broad/extended gas disk on only one side. Based on their low-density surroundings and small projected distance (<80 kpc) at a similar redshift, we conclude that tidal interaction between these two BCDs is responsible for the morphological and kinematical peculiarities in $H\small{I}$. We also investigate their star formation rates using $H{\alpha}$ and UV imaging data to probe their interaction history.
Physical properties of giant molecular clouds in the Large Magellanic Cloud
Hughes, A.,Wong, T.,Ott, J.,Muller, E.,Pineda, J. L.,Mizuno, Y.,Bernard, J.-P.,Paradis, D.,Maddison, S.,Reach, W. T.,Staveley-Smith, L.,Kawamura, A.,Meixner, M.,Kim, S.,Onishi, T.,Mizuno, N.,Fukui, Y. Blackwell Publishing Ltd 2010 Monthly notices of the Royal Astronomical Society Vol.406 No.3
<P>ABSTRACT</P><P>The Magellanic Mopra Assessment (MAGMA) is a high angular resolution <SUP>12</SUP>CO (<I>J</I>= 1 → 0) mapping survey of giant molecular clouds (GMCs) in the Large Magellanic Cloud (LMC) and Small Magellanic Cloud using the Mopra Telescope. Here we report on the basic physical properties of 125 GMCs in the LMC that have been surveyed to date. The observed clouds exhibit scaling relations that are similar to those determined for Galactic GMCs, although LMC clouds have narrower linewidths and lower CO luminosities than Galactic clouds of a similar size. The average mass surface density of the LMC clouds is 50 M<SUB>⊙</SUB> pc<SUP>−2</SUP>, approximately half that of GMCs in the inner Milky Way. We compare the properties of GMCs with and without signs of massive star formation, finding that non-star-forming GMCs have lower peak CO brightness than star-forming GMCs. We compare the properties of GMCs with estimates for local interstellar conditions: specifically, we investigate the H <SMALL>I</SMALL> column density, radiation field, stellar mass surface density and the external pressure. Very few cloud properties demonstrate a clear dependence on the environment; the exceptions are significant positive correlations between (i) the H <SMALL>I</SMALL> column density and the GMC velocity dispersion, (ii) the stellar mass surface density and the average peak CO brightness and (iii) the stellar mass surface density and the CO surface brightness. The molecular mass surface density of GMCs without signs of massive star formation shows no dependence on the local radiation field, which is inconsistent with the photoionization-regulated star formation theory proposed by McKee. We find some evidence that the mass surface density of the MAGMA clouds increases with the interstellar pressure, as proposed by Elmegreen, but the detailed predictions of this model are not fulfilled once estimates for the local radiation field, metallicity and GMC envelope mass are taken into account.</P>
Fukui, Y.,Kawamura, A.,Wong, T.,Murai, M.,Iritani, H.,Mizuno, N.,Mizuno, Y.,Onishi, T.,Hughes, A.,Ott, J.,Muller, E.,Staveley-Smith, L.,Kim, S. IOP Publishing 2009 The Astrophysical journal Vol.705 No.1
<P>We compare the CO (J = 1-0) and HI emission in the Large Magellanic Cloud in three dimensions, i.e., including a velocity axis in addition to the two spatial axes, with the aim of elucidating the physical connection between giant molecular clouds (GMCs) and their surrounding Hi gas. The CO J = 1-0 data set is from the second NANTEN CO survey and the HI data set is from the merged Australia Telescope Compact Array ( ATCA) and Parkes Telescope surveys. The major findings of our analysis are as follows: (1) GMCs are associated with an envelope of HI emission, (2) in GMCs [average CO intensity] proportional to [ average Hi intensity](1.1 +/- 0.1), and (3) the HI intensity tends to increase with the star formation activity within GMCs, from Type I to Type III. An analysis of the HI envelopes associated with GMCs shows that their average line width is 14 km s(-1) and the mean density in the envelope is 10 cm(-3). We argue that the HI envelopes are gravitationally bound by GMCs. These findings are consistent with a continual increase in the mass of GMCs via HI accretion at an accretion rate of 0.05 M-circle dot yr(-1) over a timescale of 10 Myr. The growth of GMCs is terminated via dissipative ionization and/or stellar-wind disruption in the final stage of GMC evolution.</P>