All Figures

Figure 1: Comparison of spectrum synthesis for HVS 7 (full line, best fit for abundances as in Table 1) with observations (grey), exemplary for some strategic regions. Panels  a) to  d) illustrate the and determination from Balmer lines (H in  a)) and the Si ionisation equilibrium: Si II  b), Si III  c) and Si I  d). Note the strong Si II lines in panel  b) indicative of a Si overabundance. Panel  e) illustrates the weakness (deficiency) of He I and Mg II, f) the absence (deficiency) of C II, g) the presence (strong enrichment) of Cl II and  h) a blend of Sr II and Si II. Iron group elements are highlighted in  c) and rare-earth elements in  d). Other prominent spectral lines are identified.

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In the text

Figure 2: Abundance pattern of HVS 7 (relative to solar values, Gre-vesse & Sau-val 1998) in comparison to magnetic CP stars. Symbols are identified in the legend. The error bars represent values from Table 1. Realistic errors, accounting for systematic effects (e.g. if a magnetic field were present), are expected to be larger. Upper limits are indicated by arrows. Asterisks mark abundances for the Cl-Co-rich B9p star HR 1094 (Nielsen & Wahlgren 2000) and grey bars abundance ranges observed in a sample of magnetic CP stars (López-García et al. 2001).

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In the text

	Figure 3: Position of HVS 7 in the - diagram for the determination of its evolutionary mass and age (error box in grey). Evolutionary tracks for solar metallicity are adopted from Schaller et al. (1992). Time markers in the range 130-160 Myr are shown for each track.
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In the text