Deep Galaxy counts, H I and dust at the South Galactic Pole and in the Magellanic Stream

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Abstract
Galaxy counts to B≲20mag obtained through machine measurements, atomic hydrogen column densities and IRAS data for fields around the South Galactic Pole (SGP) are intercompared. A feature in the Galaxy distribution at the SGP, which has been attributed to absorption, has no excess H I nor does there seem to be any correlation with the 100-μm flux from the faint IRAS cirrus found over much of the SGP area. The significant correlation found between H I and the 100-μm flux is consistent with a gas-to-dust ratio for the cirrus at the SGP similar to that normally associated with the Galaxy. With the present models, the IRAS data correspond to a maximum variation in reddening E(B–V) at the SGP of about 0.02 mag, with an average of only about 0.002–0.005 mag over the area of 135 deg2 investigated. Finally, despite the presence of large amounts of gas in the Magellanic Stream, we detected no associated IRAS 100-μm flux, indicating that the Stream has a different dust content from that of the gas in the Galaxy.

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