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We analyse high signal‐to‐noise ratio spectrophotometric observations acquired simultaneously with TWIN, a double‐arm spectrograph, from 3400 to 10 400 Å of three star‐forming regions in the H  ii  galaxy SDSS J165712.75+321141.4. We have measured four line temperatures –  T  e  ([O  iii ]),   T  e  ([S  iii ]),   T  e  ([O  ii ]) and   T  e  ([S  ii ]) – with high‐precision, rms errors of the order of 2, 5, 6 and 6 per cent, respectively, for the brightest region, and slightly worse for the other two. The temperature measurements allowed the direct derivation of ionic abundances of oxygen, sulphur, nitrogen, neon and argon.  We have computed  cloudy  tailor‐made models which reproduce the O  2 +  ‐measured thermal and ionic structures within the errors in the three knots, with deviations of only 0.1 dex in the case of O  +   and S  2 +   ionic abundances. In the case of the electron temperature and the ionic abundances of S  +  /H  +  , we find major discrepancies which could be the consequence of the presence of colder diffuse gas. The star formation history derived using  starlight  shows a similar age distribution of the ionizing population among the three star‐forming regions. This fact suggests a similar evolutionary history which is probably related to the process of interaction with a companion galaxy that triggered the star formation in the different regions almost at the same time. The hardness of the radiation field mapped through the use of the softness parameter  η  is the same within the observational errors for all three regions, implying that the equivalent effective temperatures of the radiation fields are very similar for all the studied regions of the galaxy, in spite of some small differences in the ionization state of different elements.  Regarding the kinematics of the galaxy, the gas rotation curve shows a deviation from the circular motion probably due either to an interaction process or to an expanding bubble or shell of the ionized gas approaching us. A dynamical mass of 2.5 × 10  10    M ⊙   is derived from the rotation curve.

Abundance determination of multiple star‐forming regions in the H ii galaxy SDSS J165712.75+321141.4