Other
Scientific paper
Dec 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993aas...183.7608c&link_type=abstract
American Astronomical Society, 183rd AAS Meeting, #76.08; Bulletin of the American Astronomical Society, Vol. 25, p.1412
Other
Scientific paper
The corotation resonance of the two-armed spiral pattern in the disk of NGC 4321 has been located. To find the resonance, we studied the kinematics of Hα -emitting gas as a tracer of gas motion in the disk of the galaxy. The Hα emission line data cube was obtained using the TAURUS-II imaging Fabry-Perot interferometer on the WHT at La Palma in 1988. The kinematic data were fitted with functions that describe circular rotation plus a perturbation due to a spiral density wave from linear theory. Our kinematic analysis shows that the corotation resonance is within the range 101--128arcsec radius. Analysis of the data is made difficult by the declining signal-to-noise beyond this radius and especially by the presence of substructure in the velocity field caused by spurs, bridges, and other strong features not part of the two-armed spiral pattern. The largest velocity perturbations caused by these extra features reach 60--80kms(-1) in the plane of the disk. The kinematically-derived location of the corotation resonance agrees with prior assertions by Elmegreen, Elmegreen, & Seiden (1989) and Elmegreen, Elmegreen, & Montenegro (1992) that the resonance is at 118arcsec radius. Those works were based on identifying resonances with azimuthally symmetric surface brightness variations. Our kinematic verification of the resonance location in NGC 4321 suggests that the symmetrized surface brightness method for locating resonances has merit.
Allen Rosalind J.
Canzian Blaise
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