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	Figure 1: The E140H spectrum of  Cen A obtained on 1999 Feb. 12. Important spectral features are marked.
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In the text

Figure 2: Blow-up of the regions containing the S V 1199.134 Å line (panel a)), the O V 1218 & 1371 Å lines (panels b) and c)), and the Fe IV quadruplet between 1601.5 and 1606.5 Å (panel  d)). Of this quadruplet we could measure only the 1602 Å line. Light-ink labels in panel  d) indicate the positions of the missed Fe IV lines. The symbol * in panels  a) and  c) marks the absorption components due to the interstellar medium. In all of the panels the wavelength scale has been shifted according to the stellar radial velocity.

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In the text

	Figure 3: A double-peak structure identified as the S I at 1241.9 Å and the Fe XII 1242 Å lines.
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In the text

	Figure 4: Plots of interesting portions of the  Cen A HST/STIS and solar SMM/UVSP spectra, the latter shifted of -2e-12 erg s-1 cm-2 Å-1. Important spectral features are marked.
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In the text

	Figure 5: The Si III, N V, Si IV, and C IV line profiles. The narrow and broad dashed lines indicate the narrow and broad Gaussian components, respectively, required to best fit the broad wings of these transition region lines. The vertical solid and dashed lines indicate the centroids of the narrow and broad Gaussians, respectively.
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In the text

	Figure 6: Doppler shifts of chromospheric and transition region lines of  Cen A relative to the photospheric radial velocity as a function of the temperature of line formation. The solid line represents a fourth order polynomial fit to the data. The dotted and dashed lines are fits to the Doppler shifts for a solar active region and the quiet Sun, respectively, by Teriaca et al. (1999).
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In the text

Figure 7: Nonthermal velocities of chromospheric and transition region lines as function of the temperature of line formation. The solid line represents a third order polynomial fit to the data. Lines which are possibly affected by opacity (Fe II, Si II, and C II) are not included in the polynomial fit ( square data points). The dotted and dashed lines represent the nonthermal line widths in a solar active region and in the quiet Sun, respectively, as derived by Teriaca et al. (1999).

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In the text

	Figure 8: Ratios of the solar to  Cen A line widths versus the temperatures of line formation.
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In the text

	Figure 9: Ratios of the solar to  Cen A line surface fluxes versus the temperatures of line formation. The * label identifies the Si II lines at 1526 and 1533 Å.
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In the text

Figure 10: Plots of interesting portions of the  Cen A HST/STIS and SOHO/SUMER quiet sun, coronal hole and solar spot spectra, shifted of -25, -35, and +50 in units of the y-axis, respectively (except for the bottom-left panel where the solar spot spectrum is shifted of +20 units). The line identified in the  Cen A STSI spectrum are labelled, while those identified on the Sun by Curdt et al. (2001) are marked with vertical lines above the quiet Sun spectrum.

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In the text

	Figure 11: The L-function curves (as defined by Landi & Landini 1998) plotted for the O IV, S IV, and O V 1218 and 1371 Å lines observed in the STIS spectrum of  Cen A.
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In the text

	Figure 12: The differential emission measure distribution of  Cen A (solid thick line) is compared with corresponding distributions for the quiet Sun and active Sun. The intersystem lines of O III 1666 Å, and of the O IV UV 0.01 multiplet near 1400 Å match the differential emission measure distribution for electron density of  [cm-3]. The Chandra X-ray data are from Raassen et al. (2003).
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In the text

	Figure 13: The S IV] 1406 Å line (panel a)) and the N IV] 1486 Å line (panel  b)) discussed in Sect. 7.
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In the text