6. Organization of the library

The corrected spectra have finally been composed into the unified library shown in Fig. 19 (click here). In this library, model spectra are given for a parameter grid which is uniformly sampled in , , and [M/H], each spectrum being available for the same wavelength grid, (), with a medium resolution of .

  
Figure 16: Bolometric correction, BC_V, as a function of effective temperature, for corrected K-library solar-metallicity dwarf model spectra. The solid line represents the empirical calibration given by Schmidt-Kaler (1982)

  
Figure 17: Residuals between differential colors obtained from original and corrected library spectra for models of the same effective temperatures and surface gravities but different metallicities. The abscissa represents the monotonic increase in temperature (as indicated along the top of the panel) and surface gravity in a similar way as Table 2 (click here). Residuals are for the coolest models from the K-library and for metallicities [M/H]=-3.0 (solid line), [M/H]=-2.0 (long-dashed line), and [M/H]=+1.0 (dotted line)

  
Figure 18: Same as Fig. 17 (click here), but for the M-giant models from the -library and for metallicities [M/H]=-1.0 (solid line) and [M/H]=+0.5 (dotted line). The zero residuals for U-B are due to the fact that in this wavelength range, -library spectra are available for solar metallicity only

  
Figure 19: The (, , [M/H]) parameter space covered by the present unified library. Solid lines delineate approximate boundaries of available models. -models for M-giants are confined to the metallicity range (grey part)

The main body consists of the K-library, which provides the most extensive coverage of parameter space (cf. Table 1 (click here)) down to , and which has therefore been fully implemented to this limit. The extensions to lower temperatures, , and associated lower surface gravities, , are provided by the M-giant spectra from the -library, which, however, covers only the limited metallicity range .

This unified library is available (in electronic form) at the CDS, Strasbourg, France, where it can be obtained in either of two versions, with the corrected or the original uncorrected spectra from the K- and -libraries.