Volume 527, March 2011
|Number of page(s)||23|
|Published online||31 January 2011|
The WSRT Virgo H i filament survey
I. Total power data⋆
Laboratoire d’Astrophysique de Marseille,
38 Rue Frédérique Joliot-Curie,
Marseille Cedex 13,
2 Kapteyn Astronomical Institute, PO Box 800, 9700 AV Groningen, The Netherlands
3 CSIRO – Astronomy and Space Science, PO Box 76, Epping, NSW 1710, Australia
Received: 11 March 2010
Accepted: 10 December 2010
Context. Observations of neutral hydrogen can provide a wealth of information about the kinematics of galaxies. To learn more about the large-scale structures and accretion processes, the extended environment of galaxies have to be observed. Numerical simulations predict a cosmic web of extended structures and gaseous filaments.
Aims. To observe the direct vicinity of galaxies, column densities have to be achieved that probe the regime of Lyman limit systems. Typically, H i observations are limited to a brightness sensitivity of NHI ~ 1019 cm-2, but this has to be improved by ~2 orders of magnitude.
Methods. With the Westerbork Synthesis Radio Telescope (WSRT), we mapped the galaxy filament connecting the Virgo Cluster with the Local Group. About 1500 square degrees on the sky was surveyed with Nyquist sampled pointings. By using the WSRT antennas as single-dish telescopes instead of the more conventional interferometer, we were very sensitive to extended emission. The survey consists of a total of 22 000 pointings, and each pointing was observed for two minutes with 14 antennas.
Results. We reached a flux sensitivity of 16 mJy beam-1 over 16 km s-1, corresponding to a brightness sensitivity of NHI ~ 3.5 × 1016 cm-2 for sources that fill the beam. At a typical distance of ten Mpc probed by this survey, the beam extent corresponds to about 145 kpc on linear scale. Although the processed data cubes are affected by confusion owing to the very large beam size, we can identify most of the galaxies that have been observed in HIPASS. Furthermore we made 20 new candidate detections of neutral hydrogen. Several of the candidate detections can be linked to an optical counterpart. The majority of the features, however, do not show any signs of stellar emission. Their origin is investigated further with accompanying H i surveys, which will be published in follow-up papers.
Key words: galaxies: evolution / intergalactic medium
Appendix is only available in electronic form at http://www.aanda.org
© ESO, 2011
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