We have determined the local galactic extinction toward the GRB 970228 field by comparing galaxy counts in two bands in this field to those in the HDF, and by comparing the observed broad band colors of stars in the GRB 970228 field to the colors of library spectra of the same spectral type. We also estimate the extinction using the neutral hydrogen column density and the amount of infrared dust emission toward this field. Combining the results of these methods, we find a best-fit galactic extinction in the optical of AV=1.09+0.10-0.20, which implies a substantial dimming and change of the spectral slope of the intrinsic GRB 970228 afterglow. Further details can be found in Castander & Lamb (1998, 1999a); see also González et al. (1999).
Re-analyzing the HST images, we measure a color for the extended source. We constrain the
nature of the likely host galaxy of GRB 970228 by comparing this color
to those obtained from synthetic galaxy spectra computed with PEGASE
(Fioc & Rocca-Volmerange 1997), taking into account the measured
extinction. The top panel of Fig. 1 shows the expected colors of an Sa, an
Sc and an Irregular galaxy with and without evolution included. Galaxies
are only consistent with the observed color if they are at high
redshift (
), or have active star formation (like the
evolving Irr shown).
The bottom panel of Fig. 1 better illustrates this point. It
shows that on-going bursts of star formation of duration shorter than 1
Gyr produce acceptable V606-I814 colors; longer duration bursts
are disfavored for redshifts . If we include the H
and K magnitudes of
Fruchter et al. (1998)
in our analysis, our
conclusions are strengthened (see
Castander & Lamb 1999b
for further details). We conclude that the host galaxy must be undergoing star
formation, in agreement with our earlier result
(Castander & Lamb 1998;
see also
Castander & Lamb 1999b).
If there is
any extinction present due to the host galaxy, this conclusion would be strengthened.
If the extended source is a galaxy with ongoing star formation, strong
emission lines are expected.
Tonry et al. (1997) and
Kulkarni et al. (1997)
have tried to obtain the spectrum of the GRB 970228
afterglow and its associated nebulosity. Neither observation revealed any obvious
emission lines. The lack of observed [OII] and Ly emission
lines suggests that the redshift of the galaxy may lie in the range
, considering the spectral coverage of the
observations.
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