UV Sounding of the M-Giant Atmosphere in the Symbiotic Binary EG-AND

Details UV Sounding of the M-Giant Atmosphere in the Symbiotic Binary EG-AND UV Sounding of the M-Giant Atmosphere in the Symbiotic Binary EG-AND

Jul 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002hst..prop.9487e&link_type=abstract

HST Proposal ID #9487

Computer Science

Hst Proposal Id #9487

Scientific paper

EG-AND is an eclipsing system which provides us with the capability to study the structure of a fairly normal non- variable red giant point-by-point through its atmosphere. The white dwarf secondary provides a bright far-UV continuum source against which absorption from a broad range of ionization levels can be seen, ranging from molecular hydrogen close to the giant star to ionized material further away. The systemic velocity is such that these features are well resolved from the intervening ISM component. In addition, the system has low extinction {A_V = 0.15}, has never been observed to undergo an eruption, and has a circular orbit, so there is no periodic disturbance of the giant atmosphere. Both calculation and direct observation show that the effect of the dwarf star's ionizing continuum on the red giant is minimal. We have an on-going FUSE program that has covered part of the orbital cycle. We have proposed for FUSE Cycle 3, and we request observing time with STIS to complete the picture. The resolution of the FUSE and STIS spectra are well-matched and suitable for detailed comparison of the intrinsic atmospheric features. Existing archival IUE data is insufficient for our purposes due to low resolution and/or low S/N. HRS data is of low S/N, partial wavelength coverage, and may suffer from instrumental scattered light. Even when both datasets are combined, some phases have never been observed in the UV.

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