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Title:
H I Distribution and Tully-Fisher Distances of Gas-Poor Spiral Galaxies in the Virgo Cluster Region
Authors:
Toribio, M. Carmen; Solanes, José M.
Affiliation:
AA(Departament d'Astronomia i Meteorologia and Institut de Ciències del Cosmos, Universitat de Barcelona. C/ Martí i Franquès, 1; E-08028 Barcelona, Spain ), AB(Departament d'Astronomia i Meteorologia and Institut de Ciències del Cosmos, Universitat de Barcelona. C/ Martí i Franquès, 1; E-08028 Barcelona, Spain )
Publication:
The Astronomical Journal, Volume 138, Issue 6, pp. 1957-1968 (2009). (AJ Homepage)
Publication Date:
12/2009
Origin:
IOP
AJ Keywords:
galaxies: clusters: individual: Virgo, galaxies: ISM, galaxies: kinematics and dynamics, galaxies: spiral, galaxies: structure, radio lines: galaxies
DOI:
10.1088/0004-6256/138/6/1957
Bibliographic Code:
2009AJ....138.1957T

Abstract

We present aperture synthesis observations in the 21 cm line of pointings centered on the Virgo Cluster region spirals NGC 4307, NGC 4356, NGC 4411B, and NGC 4492 using the Very Large Array (VLA) radio telescope in its CS configuration. These galaxies were identified in a previous study of the three-dimensional distribution of H I emission in the Virgo region as objects with a substantial dearth of atomic gas and Tully-Fisher (TF) distance estimates that located them well outside the main body of the cluster. We have detected two other galaxies located in two of our fields and observed bands, the spiral NGC 4411A and the dwarf spiral VCC 740. We provide detailed information of the gas morphology and kinematics for all these galaxies. Our new data confirm the strong H I deficiency of all the main targets but NGC 4411B, which is found to have a fairly normal neutral gas content. The VLA observations have also been used to discuss the applicability of TF techniques to the five largest spirals we have observed. We conclude that none of them is actually suitable for a TF distance evaluation, whether due to the radical trimming of their neutral hydrogen disks (NGC 4307, NGC 4356, and NGC 4492) or to their nearly face-on orientation (NGC 4411A and B).
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