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Astron. Astrophys. 318, L67-L70 (1997)

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3. Results

The results of SBS 1520+530 photometry are given in Table 1, where relative (with respect to component A) positions of four components and B, V, R, I magnitudes are presented. We had earlier discovered the three components A, B and NW; SE the faintest one, was discovered on deep V, R and I integrated images. The accuracy of relative positions is about 0:0005. All parameters of the components were derived from the direct image fitting by a set of two-dimensional Gaussian profiles. We could not find any other extended features in its neighborhood.


[TABLE]

Table 1. Relative positions and photometry of SBS 1520+530 components


The spectra of the A and B components, obtained with the 6m telescope, are shown in Fig. 2, where the ordinate is expressed in energy units. The axis designations for A and B components are presented on the left and right sides of the figure. The strongest emission lines and two absorption systems are marked.

The parameters of emission and absorption lines were derived using the Gaussian approximation of profiles. The observed wavelength and redshift of the emission lines are presented in Table 2.


[TABLE]

Table 2. Identification of emission lines in spectra of SBS 1520+530 A & B components


Using the spectral data, we could identify reliably two absorption line systems with the same redshifts ([FORMULA] =0.715, 0.815) in the spectra of each of the two components. All identified lines together with the observed wavelength and obtained redshift are given in Table 3.


[TABLE]

Table 3. Absorption lines in the [FORMULA] = 0.7155 and 0.8147 systems towards SBS 1520+530 A & B components


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© European Southern Observatory (ESO) 1997

Online publication: July 3, 1998
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