NGC 4736 H II regions properties (Martin+ 1997)

Details NGC 4736 H II regions properties (Martin+ 1997) NGC 4736 H II regions properties (Martin+ 1997)

Sep 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996ycat..33210363m&link_type=abstract

VizieR On-line Data Catalog: J/A+A/321/363. Originally published in: 1997A&A...321..363M

Computer Science

H Ii Regions, Galaxies: Ring

Scientific paper

Results of imaging spectrophotometry in the nebular lines Hα, Hβ, [O III]λ5007 and [N II]λ6584 of 65 H II regions in the early-type ringed galaxy NGC 4736 are presented. The oxygen abundance is derived using the line ratios [O III]/Hβ and [N II]/[O III] as calibrated by Edmunds & Pagel (1984MNRAS.211..507E). Analysis of the O/H distribution in the bright resonance ring of star formation in NGC 4736 reveals that the O/H scatter is similar to that of the ISM of the disc of gas-rich galaxies, despite the very high star formation rate presently observed in the ring. The magnitude of azimuthal mixing induced by supernovae explosions and galaxy differential rotation is estimated in the ring; it is found that both can explain the small O/H dispersion observed in this structure. The radial distribution of O/H in the disc of NGC 4736 is also studied. Although the number of H II regions located outside the ring, and for which a reliable O/H value was obtained is limited, a slope for the global gradient is derived and found to be moderate (~-0.035+/-0.020dex/kpc). This gradient is shallower than gradients observed in normal galaxies, and is comparable to the slopes found for galaxies with bars of medium strength. Two evolutionary scenarios are proposed to explain this O/H distribution: i) Oval distortions, like bars, induce large-scale gas flows throughout the disc of NGC 4736, resulting in radial mixing of the chemical composition on a relatively short time scale (<=1Gyr) ii) A strong bar was present in the recent past and has flattened the abundance gradient. (2 data files).

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