All Figures

Figure 1: V-band image obtained at the 3.6 m ESO telescope on 23 February 2002 of the GRB 000214 field. The BeppoSAX NFI error box (solid circle) of the GRB 000214 X-ray afterglow (Antonelli et al. 2000a) and a section of the IPN annulus (area inside the solid lines; Hurley & Feroci 2000) are reported. The NFI error circle radius is 50 with a statistical confidence level of 90%. The numbered objects show the potential candidates for the GRB 000214 host, displayed in Table 3. Candidate #1 is slightly outside ( ) and #3 is on the edge of the NFI error circle. The stars labeled as A, B, C represent the secondary standards indicated in Table 2.

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In the text

Figure 2: The plot shows the R-band magnitude of 32 GRB host galaxies (rhomboids) and the potential four hosts of GRB 000214 (squares) as a function of redshift. All the magnitudes were corrected for Galactic reddening. The four candidates were labeled following the numeration given in Table 3. The error bars of our four candidates are smaller than the size of their symbols. The curves represent the R-band magnitude evolution of a typical galaxy with redshift. The two vertical lines display the X-ray 0.37-0.47 redshift bin. The K-corrections of the curves were carried out for two spectral indexes; (upper, dashed curve) and (lower, dotted curve). The area above both non-solid curves qualitatively indicates the region populated by subluminous galaxies. As can be seen, most of the hosts (including the four candidates) tend to be subluminous galaxies. The positions of the candidates are consistent with the loci of typical host galaxies at similar redshifts (). All the magnitudes were corrected for foreground Galactic extinction, using the Schlegel et al. (1998) dust maps.

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In the text

Figure 3: Synthetic SEDs calculated by HyperZ for the four potential candidates for the GRB 000214 host galaxy. The synthetic spectra are shown by the line and the dots denote the UBVRI-band fluxes. The horizontal error bars indicate the FWHM of each filter. The detection upper limits are represented by vertical error bars ranging from the limiting flux (see the associated limiting magnitude in the column of Table 1) to zero (a more detailed description of the upper limits used by HyperZ can be found in Bolzonella et al. 2000). The inferred values of the photometric redshift, age of the dominant stellar population, and extinction are given as inserts in the corresponding panels.

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In the text