Slit observations and empirical calculations for H ii regions

Abstract

When analysing H II regions, a possible source of systematic error on empirically derived quantities, such as the gas temperature and the chemical composition, is the limited size of the slit used for the observations. In order to evaluate this type of systematic error, we use the photoionization code AANGABA to create a virtual photoionized region and mimic the effect of a slit observation. A grid of models was built varying the ionizing radiation spectrum emitted by a central stellar cluster, as well as the gas abundance. The calculated line surface brightness was then used to simulate slit observations and to derive empirical parameters using the usual methods described in the literature. Depending on the fraction of the object covered by the slit, the empirically derived physical parameters and chemical composition can be different from those obtained from observations of the whole object. This effect is mainly dependent on the age of the ionizing stellar cluster. The low-ionization lines, which originate in the outer layers of the ionized gas, are more sensitive to the size of the area covered by the slit than the highionization forbidden lines or recombination lines, because these lines are mainly produced closer to the inner radius of the nebula. For a slit covering 50 per cent or less of the total area, the measured [O III], [O II] and [O I] line intensities are less than 78, 62 and 58 per cent of the total intensity for a young H II region (t < 3 Myr); for older objects the effect due to the slit is less significant. Regarding the temperature indicator T [O III] , the slit effects are small (usually less than 5 per cent) because this temperature is derived from [O III] high-ionization lines. On the other hand, for the abundance (and temperature) indicator R 23 , which depends also on the [O II] line, the slit effect is slightly higher. Therefore, the systematic error due to slit observations on the O abundance is low, being usually less than 10 per cent, except for H II regions powered by stellar clusters with a relative low number of ionizing photons between 13.6 and 54.4 eV, which create a smaller O ++ emitting volume. In this case, the systematic error on the empirical O abundance deduced from slit observations is more than 10 per cent when the covered area is less than 50 per cent. method (with some improvements) is very convenient for obtaining a first evaluation of the chemical composition of large samples of objects such as planetary nebulae, H II regions and active galactic nuclei. The emitting gas is assumed to have high-and low-ionized zones, characterized by the temperature indicated, respectively, by the [O III] and [N II] line intensity ratios. The electron density is usually derived from the [S II] line ratio (see, for instance, Osterbrock 1989). The various ions of the elements present in the gas are assumed to be in either of these regions, following their ionization potential.As photoionization codes became friendly and available to users (such as the well-known CLOUDY), several authors...

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