This μ BA indicates that B is amplified (relative to A) by a factor of about 3 −5, with larger amplifications at shorter wavelengths. (4) The continuum flux ratio was appropriately corrected to obtain the microlensing magnification ratio of the continuum μ BA. They were used to constrain the macrolens flux ratio M BA and dust extinction parameters. (3) We determined the flux ratio B/ A for the cores of the emission lines in the two quasar spectra. (2) The spectrum of G is typical for early-type galaxies, and we measured its redshift (0.609 ± 0.001) for the first time. The new position angle for G is separated by ~50 ° from the previously determined value. Our observations led to the following main results: (1) We obtained new accurate positions for B and G (relative to A), as well as structure parameters for the light distribution of G. This consists of two images of a lensed quasar, A and B, and a lensing galaxy G between the two quasar images. We present deep I-band imaging (NOT-ALFOSC) and spectroscopic (GTC-OSIRIS) observations of the gravitational lens system SDSS J1339+1310. de Los Castros s/n, 39005 Santander, SpainĮ-mail: Institute for Radiophysics and Electronics, National Academy of Sciences of Ukraine, 12 Proskura St., 61085 Kharkov, Ukraine Goicoechea 1ġ Departamento de Física Moderna, Universidad de Cantabria, Avda. Astronomical objects: linking to databases.Including author names using non-Roman alphabets.Suggested resources for more tips on language editing in the sciences

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