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Description
We present a non-parametric cell-based method of selecting highly pure and largely complete samples of spiral galaxies using photometric and structural parameters as provided by standard photometric pipelines and simple shape fitting algorithms. The performance of the method is quantified for different parameter combinations, using purely human-based classifications as a benchmark. The discretization of the parameter space allows a markedly superior selection than commonly used proxies relying on a fixed curve or surface of separation. Moreover, we find structural parameters derived using passbands longwards of the g band and linked to older stellar populations, especially the stellar mass surface density mu_*_ and the r band effective radius r_e_, to perform at least equally well as parameters more traditionally linked to the identification of spirals by means of their young stellar populations, e.g. UV/optical colours. In particular the distinct bimodality in the parameter mu_*_, consistent with expectations of different evolutionary paths for spirals and ellipticals, represents an often overlooked yet powerful parameter in differentiating between spiral and non-spiral/elliptical galaxies. We use the cell-based method for the optical parameter set including r_e_ in combination with the Sersic index n and the i-band magnitude to investigate the intrinsic specific star-formation rate - stellar mass relation ({psi}_*_-M_*_) for a morphologically defined volume limited sample of local universe spiral galaxies. The relation is found to be well described by {psi}_*_{propto}M_*_^-0.5^ over the range of 10^9.5^M_{sun}_<=M_*_<=10^11^M_{sun}_ with a mean interquartile range of 0.4dex. This is somewhat steeper than previous determinations based on colour-selected samples of star-forming galaxies, primarily due to the inclusion in the sample of red quiescent disks.
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