1. RRI Digital Repository
  2. 04. Astronomy and Astrophysics
  3. Research Papers (A&A)
Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/2504
Full metadata record
DC FieldValueLanguage
dc.contributor.authorAngiras, R.A.-
dc.contributor.authorJog, C.J.-
dc.contributor.authorOmar, A.-
dc.contributor.authorDwarakanath, K.S.-
dc.date.accessioned2007-05-28T06:20:58Z-
dc.date.available2007-05-28T06:20:58Z-
dc.date.issued2006-07-
dc.identifier.citationMonthly Notices of the Royal Astronomical Society, 2006, Vol.369, p1849-1857en
dc.identifier.issn0035-8711-
dc.identifier.urihttp://hdl.handle.net/2289/2504-
dc.descriptionRestricted Access. An open-access version is available at arXiv.org (one of the alternative locations)en
dc.description.abstractThe HI 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 HI spatial distribution. The lopsidedness is quantified by the Fourier amplitude A1 of the m = 1 component normalized to the average value. It is also shown that in the radial region where the stellar disc and HI overlap, their A1 coefficients are comparable. All the galaxies studied show significant lopsidedness in HI. The mean value of A1 in the inner regions of the galaxies (1.5-2.5 scalelengths) is >= 0.2. This value of A1 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 (A1 >= 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 HI disc is due to its response to the halo asymmetry.en
dc.format.extent448896 bytes-
dc.format.mimetypeapplication/pdf-
dc.language.isoenen
dc.publisherBlackwell Publishing for the Royal Astronomical Societyen
dc.relation.urihttp://adsabs.harvard.edu/cgi-bin/bib_query?2006MNRAS.369.1849Aen
dc.relation.urihttp://arxiv.org/abs/astro-ph/0604120en
dc.relation.urihttp://dx.doi.org/10.1111/j.1365-2966.2006.10418.xen
dc.rights2006 Royal Astronomical Societyen
dc.subjectgalaxies: evolutionen
dc.subjectgalaxies: ISMen
dc.subjectgalaxies: spiralen
dc.subjectgalaxies: structureen
dc.titleOrigin of disc lopsidedness in the Eridanus group of galaxiesen
dc.typeArticleen
Appears in Collections:Research Papers (A&A)

Files in This Item:
File Description SizeFormat 
2006 MNRAS V369 p1849.pdf
  Restricted Access		Restricted Access438.38 kBAdobe PDFView/Open Request a copy
Show simple item record


Items in RRI Digital Repository are protected by copyright, with all rights reserved, unless otherwise indicated.