2003/11/17 by Felix J. Lockman
Physics and Astronomy · #Astrobiology #Astronomy #Astrophysical Phenomena and Observations #Astrophysics #Astrophysics and Star Formation Studies #Computer science #Galaxy #Geology #Interstellar medium #Muck #Peering #Physics #Stellar, planetary, and galactic studies #World Wide Web #astro-ph
paper · pdf · doi:10.1007/978-1-4020-2564-8_13
11 pages includes 4 figures. To appear in "Soft X-ray Emission from Clusters of Galaxies and Related Phonomena", ed. R. Lieu, Klewer
arxiv created 2003/11/17 · openalex publication_date 2004/01/01 · arxiv updated 2016/01/27 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
This paper considers some effects of foreground Galactic gas on radiation received from extragalactic objects, with an emphasis on the use of the 21cm line to determine the total N(HI). In general, the opacity of the 21cm line makes it impossible to derive an accurate value of N(HI) by simply applying a formula to the observed emission, except in directions where there is very little interstellar matter. The 21cm line can be used to estimate the likelihood that there is significant molecular hydrogen in a particular direction, but carries little or no information on the amount of ionized gas, which can be a major source of foreground effects. Considerable discussion is devoted to the importance of small-scale angular structure in HI, with the conclusion that it will rarely contribute significantly to the total error compared to other factors (such as the effects of ionized gas) for extragalactic sight lines at high Galactic latitude. The direction of the Hubble/Chandra Deep Field North is used as an example of the complexities that might occur even in the absence of opacity or molecular gas.