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For refcode 2009AJ....138.1741C:
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2009AJ....138.1741C VLA Imaging of Virgo Spirals in Atomic Gas (VIVA). I. The Atlas and the H I Properties Chung, Aeree; van Gorkom, J. H.; Kenney, Jeffrey D. P.; Crowl, Hugh; Vollmer, Bernd Abstract. We present the results of a new VLA H I Imaging survey of Virgo galaxies, the VLA Imaging survey of Virgo galaxies in Atomic gas (VIVA). The survey includes high-resolution H I data of 53 carefully selected late type galaxies (48 spirals and five irregular systems). The goal is to study environmental effects on H I gas properties of cluster galaxies to understand which physical mechanisms affect galaxy evolution in different density regions, and to establish how far out the impact of the cluster reaches. As a dynamically young cluster, Virgo contains examples of galaxies experiencing a variety of environmental effects. Its nearness allows us to study each galaxy in great detail. We have selected Virgo galaxies with a range of star formation properties in low to high density regions (at projected distances from M87, d_87_ = 0.3-3.3 Mpc). Contrary to previous studies, more than half of the galaxies in the sample (~60%) are fainter than 12 mag in B_T_ . Overall, the selected galaxies represent the late type Virgo galaxies (S0/a to Sd/Irr) down to m_p_ <~ 14.6 fairly well in morphological type, systemic velocity, subcluster membership, H I mass, and deficiency. The H I observations were done in C short (CS) configuration of the VLA radio telescope, with a typical spatial resolution of 15" and a column density sensitivity of ~3-5 x 10^19^ cm^--2^ in 3{sigma} per 10 km s^--1^ channel. The survey was supplemented with data of comparable quality from the NRAO archive, taken in CS or C configuration. In this paper, we present H I channel maps, total intensity maps, velocity fields, velocity dispersions, global/radial profiles, position-velocity diagrams and overlays of H I/1.4 GHz continuum maps on the optical images. We also present H I properties such as total flux (S_H I_), H I mass (M_H I_), linewidths (W_20_ and W_50_), velocity (V_H I_), deficiency (def_H I_), and size (D ^eff^_H I_ and D ^iso^_H I_), and describe the H I morphology and kinematics of individual galaxies in detail. The survey has revealed details of H I features that were never seen before. In this paper, we briefly discuss differences in typical H I morphology for galaxies in regions of different galaxy densities. We confirm that galaxies near the cluster core (d_87_ <~ 0.5 Mpc) have H I disks that are smaller compared to their stellar disks (D_H I_/D_25_ < 0.5). Most of these galaxies in the core also show gas displaced from the disk, which is either currently being stripped or falling back after a stripping event. At intermediate distances (d_87_ ~ 1 Mpc) from the center, we find a remarkable number of galaxies with long one-sided H I tails pointing away from M87. In a previous letter, we argue that these galaxies are recent arrivals, falling into the Virgo core for the first time. In the outskirts, we find many gas-rich galaxies, with gas disks extending far beyond their optical disks. Interestingly, we also find some galaxies with H I disks that are smaller compared to their stellar disks at large clustercentric distances. Key words: galaxies: clusters: general, galaxies: evolution, galaxies: interactions, galaxies: kinematics and dynamics =========================================================================== 2010AJ....139.2716C ERRATUM: "VLA Imaging of Virgo Spirals in Atomic Gas (VIVA). I. The Atlas and The H I Properties" (2009, AJ, 138, 1741) Chung, Aeree; van Gorkom, J. H.; Kenney, Jeffrey D. P.; Crowl, Hugh; Vollmer, Bernd Abstract. Table 3 and Figure 8 of our article contained some errors. In Table 3, Columns 11 and 13 have been corrected for six galaxies that are marked with an asterisk or a diamond, and footnotes have been updated. In Figure 8, the galaxy on the right side in the middle row should have read NGC 4522 not NGC 4405. The corrected Figure 8 appears below. Also, the following sentence was erroneously dropped from the acknowledgment: This work has been supported by NSF grants 00-98294 and 06-07643 to Columbia University and by grant 00-71251 to Yale University. ===========================================================================
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