Temperature relations and abundance determinations in H II regions

Most abundance determinations in H II regions, especially for extragalactic regions, are based on the use of temperature relations, usually between Te[N II] and Te[O III]. The calibration of strong-line methods also generally rely on the use of these relations. We explore here the reliability of old and new Te[N II]-Te[O III] relations, their dispersions, and their effects on the calculation of chemical abundances. In order to do so, we have compiled and analyzed in a homogeneous way a sample of 155 H II regions that have measurements of both temperatures. We find that some of the largest departures from the temperature relation are probably due to shocks affecting Te[N II]. We consider the effects of recombination in Te[N II] and of line blending in Te[O III], and find a residual dependence of the temperature relation on the degree of ionization. We provide new robust fits of the relation and show that our fits lead to better abundance determinations. Our fits are very similar to the most used temperature relation, based on a grid of photoionization models by Stasińska (1982), and variously cited as Campbell et al. (1986) or Garnett (1992).