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|Title:||Kinematics and physical conditions of H I in nearby radio sources. The last survey of the old Westerbork Synthesis Radio Telescope||Authors:||MACCAGNI, FILIPPO MARCELLO
Oosterloo, T. A.
|Issue Date:||2017||Journal:||ASTRONOMY & ASTROPHYSICS||Number:||604||First Page:||A43||Abstract:||We present an analysis of the properties of neutral hydrogen (H I) in 248 nearby (0.02 < z < 0.25) radio galaxies with S<SUB>1.4 GHz</SUB> > 30 mJy and for which optical spectroscopy is available. The observations were carried out with the Westerbork Synthesis Radio Telescope as the last large project before the upgrade of the telescope with phased array feed receivers (Apertif). The sample covers almost four orders of magnitude in radio power from log P<SUB>1.4 GHz</SUB> = 22.5 W Hz<SUP>-1</SUP> and 26.2 W Hz<SUP>-1</SUP>. We detect H I in absorption in 27% ± 5.5% of the objects. The detections are found over the full range of radio power. However, the distribution and kinematics of the absorbing H I gas appear to depend on radio power, the properties of the radio continuum emission, and the dust content of the sources. Among the sources where H I is detected, gas with kinematics deviating from regular rotation is more likely found as the radio power increases. In the great majority of these cases, the H I profile is asymmetric with a significant blue-shifted component. This is particularly common for sources with log P<SUB>1.4 GHz</SUB> > 24 W Hz<SUP>-1</SUP>, where the radio emission is small, possibly because these radio sources are young. The same is found for sources that are bright in the mid-infrared, I.e. sources rich in heated dust. In these sources, the H I is outflowing likely under the effect of the interaction with the radio emission. Conversely, in dust-poor galaxies, and in sources with extended radio emission, at all radio powers we only detect H I distributed in a rotating disk. Stacking experiments show that in sources for which we do not detect H I in absorption directly, the H I has a column density that is lower than 3.5 × 10<SUP>17</SUP> (T<SUB>spin</SUB>/c<SUB>f</SUB>) cm<SUP>-2</SUP>. We use our results to predict the number and type of H I absorption lines that will be detected by the upcoming surveys of the Square Kilometre Array precursors and pathfinders (Apertif, MeerKAT, and ASKAP).||Acknowledgments:||The WSRT is operated by the ASTRON (Netherlands Foundation for Research in Astronomy) with support from the Netherlands Foundation for Scientific Research (NWO). This research makes use of the SDSS Archive, funding for the creation and distribution of which was provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Aeronautics and Space Administration, the National Science Foundation, the US Department of Energy, the Japanese Monbukagakusho, and the Max Planck Society. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. For this research we made extensive use of the software Karma (Gooch 1996) and TOPCAT (Taylor 2005). The research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Programme (FP/2007–2013)/ERC Advanced Grant RADIOLIFE-320745. The authors wish to thank Dr. Robert Schulz and Dr. Bradley Frank for useful discussions and suggestions.||URI:||http://hdl.handle.net/20.500.12386/30924||URL:||http://arxiv.org/abs/1705.00492v1
|Appears in Collections:||1.01 Articoli in rivista|
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checked on Sep 19, 2021
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