By P. B. W. Schwering, F. P. Israel (auth.)
Around the start of the 16th century, Portuguese and Dutch sailors first ventured into southern seas. With their prepared navigational curiosity within the skies, they famous the continual presence of 2 cloud-like good points, now not faraway from the just about instantly Southern Pole. the 1st literature point out of those 'clouds' was once within the magazine written in 1520 through the Italian navigator Pigafetta at the first circumnavigation of the globe through Magalhaes (c/. Pigafetta et ai. , 1962). In honour of this make the most, the gadgets have due to the fact turn into referred to as the Magellanic Clouds, even if the Dutch identify 'Kaapsche Wolken' (Cape Clouds - after the Cape of fine wish) has additionally been in use for hundreds of years. the massive and Small Magellanic Clouds are dwarf abnormal galaxies, orbiting our personal Milky method Galaxy, almost immediately at distances of fifty three and sixty three kpc respectively (Humphreys, 1984) . . they're the galaxies nearest to us: such a lot different neighborhood crew galaxies are of order ten occasions extra far-off. The LMC and SMC also are the prototypical blue dwarf irregulars, representatives of a category of gadgets during which a number of hundred extra far away gadgets are actually recognized. Their lots are a number of according to cent of the mass of the Milky method Galaxy, yet they're really gas-rich and seem to be, at the moment epoch, forming stars at a extra prodiguous cost than our Galaxy (c/. Lequeux, 1984).
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Additional info for Atlas and Catalogue of Infrared Sources in the Magellanic Clouds
The errors are approximately 10" - 15". The errors in positions of sources directly taken from the infrared maps are approximately 1'. Lm intensity peak and background level (in 10-8 Watt m- 2 sr- I ). A dash indicates that the source is below the intensity search level. Lm band. Lm band. Lm band. Column 7: The size of the source in a(') x 6( '). p denotes a source that cannot be discerned from a point source response. A colon denotes an uncertain size. A dash indicates that no reliable size could be estimated because no FWHM could be determined.
DEM 15Z. 6'H of LI-LMC 899. Infrared peak in Bar. On infrared gradient in between peaks. 4'5 of 965. On IR peak in Bar. See DEM 177. O'NE of LI-LMC 1070. On infrared gradient to 1076. 7'SH of 1083. 4'SE of LI-LHC 1076. 1'SE of LI-LMC 1115. At SE end of Bar. 9'N of LI-LHC 114Z. At SE end of Bar. 8'SH of LI-LMC 1171. At SE end of Bar. 7' SE of 1180). 1'E of LI-LMC 1195. On infrared extension near Bar. 8'N of lZ09. IR extension to 30 Doradus. See DEM Z3Z. 7'NH of 125Z). 5'NH of lZ70). In infrared extended emission, near GDR.
See OEM 271. 7'NE of LI-LHe 1539. In GDR. In 30 Ooradus outskirts. 7'SE of LI-LHe 1553. In GDR. 4'N of LI-LHe 1586. Infrared peak in GDR. See OEM 298. 7'5 of LI-LHe 1629. Infrared peak in GOR. See OEM 304. 3'S of 1662). 1'5 of LI-LHe 1671. On IR extension to 1643. See OEM 306. 9'NH of 1692). 7'NH of LI-LMC 1741. On IR gradient to 1743. See DEM 326. 3: Infrared emission from LMC stellar objects. (1) IZ) Catalog tUnber Infrared LI-LMC SAO stars (3) (4) Detection quality Remarks .... 3'S of LI-LHC 141S.