The WSRT Virgo HI filament survey I; Total Power Data

TL;DR

This survey uses the WSRT in total power mode to map the extended neutral hydrogen environment around galaxies, reaching unprecedented sensitivity to detect faint gaseous filaments and structures in the cosmic web.

Contribution

It introduces a novel large-scale, high-sensitivity HI survey using WSRT total power observations, probing the cosmic web at column densities two orders of magnitude lower than previous surveys.

Findings

Detected 20 new neutral hydrogen candidates.

Identified most known galaxies in the survey area.

Found features without stellar counterparts.

Abstract

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. To observe the direct vicinity of galaxies, column densities have to be achieved that probe the regime of Lyman limit systems. Typically HI observations are limited to a brightness sensitivity of NHI ~ 10^19 cm-2 but this has to be improved by ~2 orders of magnitude. With the Westerbork Synthesis Radio Telescope (WSRT) we map the galaxy filament connecting the Virgo Cluster with the Local Group. About 1500 square degrees on the sky is surveyed, with Nyquist sampled pointings. By using the WSRT antennas as single dish telescopes instead of the more conventional interferometer we are very sensitive to extended emission. The survey consists of a total of 22,000 pointings and each pointing has been observed for 2 minutes with 14 antennas. We reach a flux sensitivity of 16 mJy beam-1 over 16 km s-1, corresponding to a brightness sensitivity of NHI ~ 3.5 \times 10^16 cm-2 for sources that fill the beam. At a typical distance of 10 Mpc probed by this survey, the beam extent corresponds to about 145 kpc in linear scale. Although the processed data cubes are affected by confusion due 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 HI surveys which will be published in follow up papers.