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Table 2:

Analysis for eight stars from the HS survey, not included in Edelmann et al. (2003).

Name
\ensuremath{m_{\rm {pg}}} Class \ensuremath {T_{\rm {eff}}} \ensuremath{\log g} \ensuremath{\log y}
  mag   kK dex dex
Observed with CA/ TWIN
HS 1733+4540 15.1 sdOB 37.5 5.6 -3.0
HS 1909+7004 15.4 sdB 36.5 5.4 -2.9
Spectra courtesy of Aguilar-Sánchez (1998)
HS 0026+04391 14.8 sdB 36.7 5.8 -3.0
HS 0042+09271 16.0 sdB 30.2 5.6 -2.9
HS 2254+06401 15.2 sdB 29.1 5.6 -2.7
HS 2320+08401,2 14.6 sdB+ 30.0 5.8 -2.6
HS 2323+04591 14.8 sdB 29.3 5.4 -2.8
HS 2334+0144 15.5 sdB 30.8 5.6 -2.6

Notes.  \ensuremath{m_{\rm {pg}}} gives the photographic magnitude from the HS survey plates, ``Class'' our spectroscopic classification, followed by the effective temperature ( \ensuremath {T_{\rm {eff}}}), surface gravity ( \ensuremath{\log g}), and atmospheric helium abundance ($\log y$ =  \ensuremath{\log \left(N_{{\rm He}}/N_{{\rm H}}\right)}), from our model fits. The sdB+ classification indicates a composite spectrum. The notes on the names imply: (1) Also found in the PG survey (Green et al. 1986).
(2) Also found in the KUV survey (Noguchi et al. 1980).


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