In this paper we develop tools for observers to use when analysing nebular spectra for temperatures and metallicities, with two goals: to present a new, simple method to calculate equilibrium electron temperatures for collisionally excited line flux ratios, using the latest atomic data; and to adapt current methods to include the effects of possible non-equilibrium "κ" electron energy distributions.we find that existing methods based on older atomic data seriously overestimate the electron temperatures, even when considering purely Maxwellian statistics. If κ distributions exist in H ii regions and planetary nebulae as they do in solar system plasmas, it is important to investigate the observational consequences. This paper continues our previous work on the κ distribution (Nicholls et al. 2012). We present simple formulaic methods that allow observers to (a) measure equilibrium electron temperatures and atomic abundances using the latest atomic data, and (b) to apply simple corrections to existing equilibrium analysis techniques to allow for possible non-equilibrium effects. These tools should lead to better consistency in temperature and abundance measurements, and a clearer understanding of the physics of H ii regions and planetary nebulae.

Far-infrared and optical [O iii] lines are useful temeprature-density diagnostics of nebular as well as dust obscured astrophysical sources. Fine structure transitions among the ground state levels 1s 2 2s 2 2p 3 3 P 0,1,2 give rise to the 52 and 88 µm lines, whereas transitions among the 3 P 0,1,2 , , 1 D 2 , 1 S 0 levels yield the well-known optical lines λλ 4363, 4959 and 5007Å. These lines are excited primarily by electron impact excitation. But despite their importance in nebular diagnostics collision strengths for the associated fine structure transitions have not been computed taking full account of relativistic effects. We present Breit-Pauli R-matrix calculations for the collision strengths with highly resolved resonance structures. We find significant differences of up to 20% in the Maxwellian averaged rate coefficients from previous works. We also tabulate these to lower temperatures down to 100 K to enable determination of physical conditions in cold dusty environments such photo-dissociation regions and ultra-luminous infrared galaxies observed with the Herschel space observatory. We also examine the effect of improved collision strengths on temperature and density sensitive line ratios.

The flat band potentials and carrier densities of spin coated and sprayed MAPbI, FACsPbI, and MAPbBr perovskite films were determined using the Mott-Schottky relation. The films developed a space charge layer and exhibited p-type conduction with a carrier concentration of ∼10 cm for spin coated films. Electrochemical impedance spectra showed typical space charge impedance at frequencies >1 kHz, and an exceptional high capacitance at frequency <1 kHz owing to an ion diffusion component.

Improved collisions strengths for the mid-infrared and optical transitions in Ne v are presented. Breit-Pauli R-Matrix calculations for electron impact excitation are carried out with fully resolved near-threshold resonances at very low energies. In particular, the fine structure lines at 14 µm and 24 µm due to transitions among the ground state levels 1s 2 2s 2 2p 3 3 P 0,1,2 , and the optical/near-UV lines at 2973, 3346 and 3426Å transitions among the 3 P 0,1,2 , 1 D 2 , 1 S 0 levels are described. Maxwellian averaged collision strengths are tabulated for all forbidden transistion within the ground configuration. Significant differences are found in the low temperature range T e < 10000 K for both the FIR and the opitcal transitions compared to previous results. An analysis of the 14/24 µm ratio in low-energy-density (LED) plasma conditions reveals considerable variation; the effective rate coefficient may be dominated by the very low-energy behaviour rather than the maxwellian averaged collision strengths. Computed values suggest a possible solution to the anomalous mid-IR ratios found to be lower than theoretical limits observed from planetary nebulae and Seyfert galaxies. While such LED conditions may be present in infrared sources, they might be inconsistent with photoionization equilibrium models.