We have used the Balmer and Paschen jumps to determine the temperatures of the H+ zones of a total sample of 47 H II regions. The Balmer jump was used on MMT spectrophotometric data of 22 low-metallicity H II regions in 18 blue compact dwarf (BCD) galaxies and of one H II region in the spiral galaxy M101. The Paschen jump was used on spectra of 24 H II emission-line galaxies selected from the Data Release 3 of the Sloan Digital Sky Survey (SDSS). To derive the temperatures, we have used a Monte Carlo technique varying the electron temperature in the H+ zone, the extinction of the ionized gas and that of the stellar population, the relative contribution of the ionized gas to the total emission, and the star formation history to fit the spectral energy distribution of the galaxies. For the MMT spectra, the fit was done in the wavelength range 3200-5200 ?, which includes the Balmer discontinuity, and for the SDSS spectra, in the wavelength range 3900-9200 ?, which includes the Paschen discontinuity. We find for our sample of H II regions that the temperatures of the O2+ zones determined from the nebular-to-auroral line intensity ratio of doubly ionized oxygen [O III] λλ(4959 + 5007)/λ4363 do not differ, in a statistical sense, from the temperatures of the H+ zones determined from fitting the Balmer and Paschen jumps and the spectral energy distributions (SEDs). We cannot rule out small temperature differences of the order of 3%-5%.
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机译：我们已经使用Balmer和Paschen跳跃来确定47个H II区总样本的H +区温度。 Balmer跳跃用于MMT分光光度数据，该数据用于18个蓝色紧密矮星（BCD）星系中的22个低金属H II区和旋涡星系M101中的一个H II区。 Paschen跃迁用于从Sloan Digital Sky Survey（SDSS）的数据版本3中选出的24 H II发射线星系的光谱中。为了得出温度，我们使用了蒙特卡罗技术来改变H +区的电子温度，电离气体和恒星群体的消光，电离气体对总发射的相对贡献以及恒星形成拟合星系光谱能量分布的历史。对于MMT光谱，在包括Balmer不连续性的3200-5200λ波长范围内进行拟合，对于SDSS光谱，在包括Paschen不连续性的3900-9200λ波长范围内进行拟合。在H II区域的样本中，我们发现，由双离子氧[O III]λ+（4959 + 5007）/λ4363的神经对极光线强度比确定的O2 +区温度在统计上没有差异从H +区域的温度（通过拟合Balmer和Paschen跳跃以及光谱能量分布（SED））可以确定。我们不能排除3％-5％的小温差。
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