... dwarfs

Based on observations made with the Italian Telescopio Nazionale Galileo (TNG) operated on the island of La Palma by the Centro Galileo Galilei of the INAF (Istituto Nazionale di Astrofisica) at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias.

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...

Based on observations made with the William Herschel Telescope and Isaac Newton Telescope operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias.

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...

Tables 2-4 are available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/448/579 and at http://www.edpsciences.org

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...)

After the evaluation of the final absolute proper motion of the confirmed WDs (see Table 2), a few objects resulted moving with $\mu<0.28''$ yr^-1. This is due to the relatively large error of the short baseline proper motions (POSS-II plates only), which were used for the selection of the candidates; in some cases these are objects close to the plate edge. Also, improved photometry resulted in few objects slightly brighter than $R_{\rm F}=16$.

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... diagram

Notice that most of the objects with $H\approx 25$ are not real, and were rejected by the application of the selection criteria and visual inspection.

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... respectively

Those numbers represent mean values computed numerically assuming the velocity ellipsoids $(\sigma_U, \sigma_V, \sigma_W; v_a)=(34,21,18;-6)$ for the thin disk (Binney & Merrifield 1998, Table 10.4), (63, 39, 39; -45) for the thick disk (Soubiran et al. 2003), and (160, 89, 94; -217) for the halo (Casertano et al. 1990). Also, a solar motion (U,V,W)=(10.0, 5.25, 7.17) km s^-1 is adopted from Dehnen & Binney (1998).

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... WDs

The exact fraction of selected objects is a function of the line of sight because it depends on the projection of the velocity ellipsoid. Assuming the velocity ellipsoid from Casertano et al. (1990) and Soubiran et al. (2003) respectively for the halo and thick disk, we estimated that for our fields at intermediate galactic latitudes less than 2% of the halo WDs and 20% of the thick disk WDs are moving with $V_{\rm tan}<38$ km s^-1. Such fraction decreases to a minimum of 0.25% and 13% of halo and thick disk WDs in the cases of the high latitude fields towards the NGP.

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... sample

The spectra of the two WDs GSC2U J124212.6+295801 and GSC2U J222233.1+122140 have a reduced wavelength coverage as they were observed at the TNG with a different Grism (LR-R).

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