Halpha/FUV Intensity Ratios in the Galaxy and The Source of The Diffuse Halpha Emission

Details Halpha/FUV Intensity Ratios in the Galaxy and The Source of The Diffuse Halpha Emission Halpha/FUV Intensity Ratios in the Galaxy and The Source of The Diffuse Halpha Emission

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...211.9212s&link_type=abstract

American Astronomical Society, AAS Meeting #211, #92.12; Bulletin of the American Astronomical Society, Vol. 39, p.888

Astronomy and Astrophysics

Astrophysics

Scientific paper

We compare the far-ultraviolet (FUV; 1370-1720A) continuum and the diffuse Halpha emission maps of the Galaxy to investigate the ionizing source of the interstellar Halpha emission. The FUV continuum map was obtained with the Spectroscopy of Plasma Evolution from Astrophysical Radiation instrument (SPEAR/FIMS). The Halpha/FUV intensity ratios in the Warm Ionized Medium (WIM) are found to be in general lower than the ratios in the classical HII regions. We have directly compared the observed ratios in the WIM to the predictions from the individual in-situ stars that may dominate the lines of sight if there is no radiation field from distant stars. Furthermore, we study the relative importance of B type stars compared to O types in producing the diffuse Halpha emission. In particular, an important constraint on the contribution of O stars is placed to be < 10% toward the lines of sight where the lowest Halpha/FUV ratios are measured. It is also shown that stellar radiations from B2-B3 stars are required to explain the lowest value of the Halpha/FUV ratios. The SPEAR (FIMS) Mission is supported by NASA grant NAG5-5355 and the Korea Ministry of Science and Technology.

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