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Title:
BV photometry of five shell galaxies
Authors:
Pierfederici, F.; Rampazzo, R.
Affiliation:
AA(NOAO, 950 North Cherry Avenue, Tucson, AZ 85719, USA), AB(INAF-Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, 35122, Padova, Italy)
Publication:
Astronomische Nachrichten, Vol.325, Issue 5, p.359-375 (AN Homepage)
Publication Date:
06/2004
Origin:
AN
Keywords:
galaxies: formation, galaxies: evolution, galaxies: ellipticals and lenticulars, galaxies: interactions, galaxies: individual (NGC 470, NGC 474, NGC 6776, NGC 7010, NGC 7585, IC 1575)
DOI:
10.1002/asna.200310235
Bibliographic Code:
2004AN....325..359P

Abstract

Current views consider shell structures as bona fide signatures of a recent minor/major merging event though also weak interaction models (WIM) could produce long lasting shells on host galaxies possessing a stellar thick disc. We present a B V band photometric study of a sample of 5 shell galaxies belonging to the Malin & Carter (1983) compilation. The structural properties and colors of the galaxies, as well as the colors of their shells are examined in detail. We did not find signatures of the presence of double nuclei. NGC 7585 is the only E galaxy in the sample and has a moderately boxy structure. The other galaxies have either a discy structure or are mixed E/S0 type galaxies. NGC 474 is a true lenticular. NGC 6776 shows a diffuse asymmetric outer structure and a system of tails of the the same color of the galaxy body; but not clear shells. In general, the color of the shells in our sample is similar or slightly redder than that of the host galaxy, whose color, in turn, is typical of the early-type morphological class. One of the outer shells of NGC 474 is significantly bluer than the body of the galaxy. Since NGC 474 appears to be interacting with NGC 470, the color of this one shell could be explained as result of a recent acquisition of material through tidal interaction. The WIM hypothesis could explain both the red and the blue shells of NGC 474, this latter acquired from the fly-by of the nearby companion NGC 470, but the lack of the constancy of shell surface brightness as a ratio of the underlying galaxy brightness argues against WIM. We speculate about evidence, which also comes from different observations, that suggests a merging/accretion origin of the shells.

Based on observations obtained at the Observatoire de Haute Provence, CNRS, Saint Michel l'Observatoire, France and ESO, La Silla, Chile

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