593. Serendipitous EUV Sources Detected during the First Year of the Extreme Ultraviolet Explorer Right Angle Program (McDonald, et al. 1994)

K. McDonald, N. Craig, M.M. Sirk, J.J. Drake, A. Fruscione, J.V. Vallerga, and R.F. Malina, Astron. J., 108, 1843-1853, 1994.

Abstract

Paper

• Text (PostScript)

Tables

• Table 1: 10% Filter Bandpasses (see Paper)
• Table 2: EUVE Right Angle Program Source List ( text or PostScript )
• Table 3: Breakdown of RAP Source List by Spectral Type (see Paper)

Figures

• Figure 1 (PostScript) : Adopted UV effective areas for Lexan/B filter/detector systems of EUVE scanning telescopes based on measurements of the sunlit Earth and Moon (curves) and ground-based UV throughput measurements at specific wavelengths (open symbols). Note that the throughput for Scanner B is about 20 times lower than that for Scanner A at 2537 Å.
• Figure 2: Figure 2a (PostScript) shows the Lexan/B count rates derived from data collected by Scanner A for 60 detected B stars from the EUVE all-sky survey vs. their visual magnitude. The filled squares represent B stars with spectral type B0 through B3, while the open squares represent spectral type B5 through B9.5. Figure 2b (PostScript) plots the same for the data collected by Scanner B. Note that the sensitivity to UV photons is much higher for Scanner A than for Scanner B. The open triangle represents the count rate for HR 2875 (B5Vp), the only B star detected in both the Al/Ti/C and Lexan/B bandpasses during the RAP. Note also that beta Per shows an anomalously high Lexan/B count rate for a later type B star, indicating that some of these photons result from EUV flux from this interacting binary system.