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Date and Time of the Query: 2019-07-20 T07:45:19 PDT
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For refcode 2006MNRAS.369.1849A:
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NED Abstract

Copyright by Royal Astronomical Society. 2006MNRAS.369.1849A Origin of disc lopsidedness in the Eridanus group of galaxies Angiras, R. A.; Jog, C. J.; Omar, A.; Dwarakanath, K. S. Abstract. The H I surface density maps for a sample of 18 galaxies in the Eridanus group are Fourier analysed. This analysis gives the radial variation of the lopsidedness in the H I spatial distribution. The lopsidedness is quantified by the Fourier amplitude A_1_ of the m = 1 component normalized to the average value. It is also shown that in the radial region where the stellar disc and H I overlap, their A_1_ coefficients are comparable. All the galaxies studied show significant lopsidedness in H I. The mean value of A_1_ in the inner regions of the galaxies (1.5-2.5 scalelengths) is >= 0.2. This value of A_1_ is twice the average value seen in the field galaxies. Also, the lopsidedness is found to be smaller for late-type galaxies; this is opposite to the trend seen in the field galaxies. These two results indicate a different physical origin for disc lopsidedness in galaxies in a group environment compared to the field galaxies. Further, a large fraction (30 per cent) shows a higher degree of lopsidedness (A_1_>= 0.3). It is also seen that the disc lopsidedness increases with the radius as demonstrated in earlier studies, but over a radial range that is two times larger than done in the previous studies. The average lopsidedness of the halo potential is estimated to be 10 per cent, assuming that the lopsidedness in H I disc is due to its response to the halo asymmetry. Key words: galaxies: evolution,galaxies: ISM,galaxies: spiral,galaxies: structure
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