Survey1
N. M. McClure-Griffiths ,
John M. Dickey ,
B. M. Gaensler ,
A. J. Green ,
R. F. Haynes ,
M. H. Wieringa
, PASA, 18 (1), in press.
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Title/Abstract Page: H I Emission and Absorption
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Questions and Future Work
There are several questions to be answered about the H I shells and H I self-absorption as we proceed with the SGPS. With the SGPS dataset we expect to catalogue many new shells. How are these shells distributed in the Galaxy? Do they lie along spiral arms like GSH 277+0+36 and GSH 280+0+59, or is their distribution seemingly random as in the Large and Small Magellanic Clouds (Kim et al. 1998; Staveley-Smith et al. 1997)? How large an impact do shells have on the global ISM? Will the Milky Way resemble the LMC and SMC which are dominated by shells? With respect to the small scale structure, we ask: How are the HISA features distributed? Do they lie predominantly along spiral shocks or are they ubiquitous? How do they relate to the molecular clouds? What fraction of the ISM is in the CNM? Are there larger, warmer clouds that we are missing? How small are the numerous clouds that remain unresolved by the SGPS?Next Section: Conclusions
Title/Abstract Page: H I Emission and Absorption
Previous Section: H I Self-Absorption (HISA)
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