``The Local Volume HI Survey'' (LVHIS) is a project comprising deep HI line and 20-cm radio continuum observations for all nearby, gas-rich galaxies, supplemented by multi-wavelength data.
Our initial sample consists of all galaxies with vLG < 550 km/s or D < 10 Mpc that are detected in the `HI Parkes All-Sky Survey' (HIPASS). A declination limit of DEC < -30 degrees was chosen for observations with the Australia Telescope Compact Array (ATCA). For LV galaxies with DEC > +20 degrees with used the Westerbork Radio Synthesis Telescope, see the WSRT-LVHIS project. Similar projects are also under way at the VLA and the GMRT.
If you are interested in a *postdoc positions* at CSIRO ATNF, please contact Baerbel.Koribalski at csiro.au .
- 3-year HI postdoc position with B. Koribalski (Job Ref - NSW13-03277; Position description; closing date: 18 Nov)
- 3-year Bolton Fellowship - Wide-field radio astronomy (Job Ref - NSW13-03372; Position description; closing date: 18 Nov)
- PhD top-up scholarships (more details soon) (Job Ref - NSW13-03xxx; Position description; closing date: xx Nov) - Further information.
LVHIS - a step towards WALLABY
LVHIS is a significant step towards the ASKAP HI All-Sky Survey (nick-named WALLABY), as it delivers similar spectral line sensitivity and resolution. WALLABY is a large survey project (approx. one-year; 8h per pointing) exploring 2/3 of the sky out to a redshift of 0.25. Combined with a WSRT Northern Sky HI Survey (WNSHS; DEC > +27 degr) we will be able to achieve a homogenous all-sky HI survey.
Our aim is to study the formation and evolution of galaxies in the Local Universe. HI spectral line (21-cm) observations allow us to trace the overall matter distribution in galaxies, measure their velocity fields and deduce their gas dynamics and morphology. The gaseous envelopes of galaxies typically extent far beyond their stellar disks. Locations of star formation can usually be identified by high density HI clumps in the outer disks. HI is also found between galaxies (e.g. in groups and clusters), high-lighting their tidal interactions as well as ram pressure stripping.
We have obtained full 12-h synthesis observations of the sample galaxies with three ATCA configurations (EW352/367-m, 750-m, and 1.5-km). For galaxies with very large HI envelopes we also obtained HI mosaics in the H75 array, the most compact ATCA configuration. These data were then used to make detailed maps of the HI distribution & HI velocity fields of the Local Volume galaxies as well as their star formation properties on all scales. Our data will be complemented by deep AAT H-band images, as well as BVRI-, Halpha-, GALEX uv- and Spitzer mid-infrared images.