Table 1: Observational parameters for narrow-band H $\alpha$ photometric observations and the TAURUS Fabry-Pérot interferometry for NGC 6951, NGC 3359 and NGC 1530. Seeing is taken as the FWHM measured in the final continuum-subtracted H $\alpha$ images of unsaturated stellar sources and the seeing for Fabry-Pérot observations is the FWHM of the continuum images obtained from the analysis of the data cubes and the spectral resolution is the velocity separation between adjacent planes in the data cube.
Narrow-band Fabry-Pérot

Filter (H $\alpha$ ) Filter (continuum) Pixel size Seeing Filter Pixel size Seeing Spect. res.

( $^{\prime \prime }$ /pix) ( $^{\prime \prime }$ ) ( $^{\prime \prime }$ /pix) ( $^{\prime \prime }$ ) (km s^-1)

NGC 6951 6589/15 6565/44 0.28 0.8 6589/15 0.58 1.3 15.63

NGC 3359 6594/44 6686/44 0.59 1.5-1.6 6589/15 0.56 1.5 15.66

NGC 1530 6626/44 HARRIS R 0.33 1.2-1.4 6613/15 0.29 1.0 18.62

**Table 1:** Observational parameters for narrow-band H $\alpha$ photometric observations and the TAURUS Fabry-Pérot interferometry for NGC 6951, NGC 3359 and NGC 1530. Seeing is taken as the *FWHM* measured in the final continuum-subtracted H $\alpha$ images of unsaturated stellar sources and the seeing for Fabry-Pérot observations is the *FWHM* of the continuum images obtained from the analysis of the data cubes and the spectral resolution is the velocity separation between adjacent planes in the data cube.
	Narrow-band	Fabry-Pérot
	Filter (H $\alpha$ )	Filter (continuum)	Pixel size	Seeing	Filter	Pixel size	Seeing	Spect. res.
			( $^{\prime \prime }$ /pix)	( $^{\prime \prime }$ )		( $^{\prime \prime }$ /pix)	( $^{\prime \prime }$ )	(km s^-1)
NGC 6951	6589/15	6565/44	0.28	0.8	6589/15	0.58	1.3	15.63
NGC 3359	6594/44	6686/44	0.59	1.5-1.6	6589/15	0.56	1.5	15.66
NGC 1530	6626/44	HARRIS R	0.33	1.2-1.4	6613/15	0.29	1.0	18.62

Source LaTeX | All tables | In the text

	1 Introduction
	2 The observations
	3 Relating the photometric and spectroscopic data sets
	4 Extraction of the line profiles
	5 Spectral analysis
	6 The luminosity v. non-thermal velocity dispersion relation
	7 The masses of the H II regions in the log L ${_{\scriptsize {\rm H \alpha}}}$ - log ${\sigma _{\rm nt}}$ diagram
	8 Conclusions
	Appendix A: The effects of different H II region size estimate criteria
	References