Ring Star Formation Rates in Barred and Nonbarred Galaxies

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dc.contributor.author Grouchy, R. D.
dc.contributor.author Buta, R. J.
dc.contributor.author Salo, H.
dc.contributor.author Laurikainen, E.
dc.date.accessioned 2019-06-12T16:12:04Z
dc.date.available 2019-06-12T16:12:04Z
dc.date.copyright 2010
dc.date.issued 2010-05-10
dc.identifier.citation Grouchy, R., Buta, R., Salo, H., Laurikainen, E. (2010): Ring Star Formation Rates in Barred and Nonbarred Galaxies. The Astronomical Journal, 139(6). DOI: 10.1088/0004-6256/139/6/2465 en_US
dc.identifier.uri http://ir.ua.edu/handle/123456789/5733
dc.description.abstract Nonbarred ringed galaxies are relatively normal galaxies showing bright rings of star formation in spite of lacking a strong bar. This morphology is interesting because it is generally accepted that a typical galactic disk ring forms when material collects near a resonance, set up by the pattern speed of a bar or bar-like perturbation. Our goal in this paper is to examine whether the star formation properties of rings are related to the strength of a bar or, in the absence of a bar, to the non-axisymmetric gravity potential in general. For this purpose, we obtained Hα emission line images and calculated the line fluxes and star formation rates (SFRs) for 16 nonbarred SA galaxies and four weakly barred SAB galaxies with rings. For comparison, we combine our new observations with a re-analysis of previously published data on five SA, seven SAB, and 15 SB galaxies with rings, three of which are duplicates from our sample. With these data, we examine what role a bar may play in the star formation process in rings. Compared to barred ringed galaxies, we find that the inner ring SFRs and Hα+[N II] equivalent widths in nonbarred ringed galaxies show a similar range and trend with absolute blue magnitude, revised Hubble type, and other parameters. On the whole, the star formation properties of inner rings, excluding the distribution of H II regions, are independent of the ring shapes and the bar strength in our small samples. We confirm that the deprojected axis ratios of inner rings correlate with maximum relative gravitational force Q_g ; however, if we consider all rings, a better correlation is found when a local bar forcing at the radius of the ring, Q_r , is used. Individual cases are described and other correlations are discussed. By studying the physical properties of these galaxies, we hope to gain a better understanding of their placement in the scheme of the Hubble sequence and how they formed rings without the driving force of a bar. en_US
dc.format.mimetype application/pdf en_US
dc.language English en_US
dc.publisher American Astronomical Society en_US
dc.subject Kinematics and dynamics en_US
dc.subject Photometry en_US
dc.subject Spiral galaxies en_US
dc.subject Structure en_US
dc.title Ring Star Formation Rates in Barred and Nonbarred Galaxies en_US
dc.type text en_US
dc.rights.holder American Astronomical Society en_US

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