Mon. Not. R. Astron. Soc., 435, 1020-1036 (2013/October-3)
Quantified HI morphology - VII. Star formation and tidal influence on local dwarf HI morphology.
HOLWERDA B.W., PIRZKAL N., DE BLOK W.J.G. and BLYTH S.-L.
Abstract (from CDS):
Scale-invariant morphology parameters applied to atomic hydrogen maps (Hi) of galaxies can be used to quantify the effects of tidal interaction or star formation on the interstellar matter (ISM). Here we apply these parameters, concentration, asymmetry, smoothness, Gini, M20, and the GM parameter, to two public surveys of nearby dwarf galaxies, the Very Large Array-ANGST and Local Irregulars That Trace Luminosity Extremes-The Hi Nearby Galaxy Survey, to explore whether tidal interaction or the ongoing or past star formation is a dominant force shaping the Hi disc of these dwarfs. Previously, Hi morphological criteria were identified for ongoing spiral-spiral interactions. When we apply these to the irregular dwarf population, they either select almost all or none of the population. We find that only the asymmetry-based criteria can be used to identify very isolated dwarfs (i.e. these have a low tidal indication). Otherwise, there is little or no relation between the level of tidal interaction and the Hi morphology. We compare the Hi morphology to three star formation rates based on either Hα, far-ultraviolet or the resolved stellar population, probing different star formation time-scales. The Hi morphology parameters that trace the inequality of the distribution, the Gini, GM, and M20 parameters, correlate weakly with all these star formation rates. This is in line with the picture that local physics dominates the ISM appearance and not tidal effects. Finally, we compare the Sloan Digital Sky Survey measures of star formation and stellar mass to the Hi morphological parameters for all four Hi surveys. In the two lower resolution Hi surveys (12arcsec), there is no relation between star formation measures and Hi morphology. The morphology of the two high-resolution Hi surveys (6arcsec), the asymmetry, smoothness, Gini, M20, and GM do show a link to the total star formation, but a weak one.
© 2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society (2013)
ISM: structure - galaxies: dwarf - galaxies: ISM - Local Group - galaxies: structure - radio lines: ISM
The bibliographic reference for Hunter et al. 2012 is 2012AJ....144..134H (not ApJ). Table 1, KKH 230 is a probable misprint for KK 230 ([KK98A] 230 in Simbad). LGC 3 is likely LGS 3.
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