The Wide Area VISTA Extra-galactic Survey (WAVES) is a 4MOST Consortium Design Reference Survey which will use the VISTA/4MOST facility to spectroscopically survey ~2million galaxies to $r_{rm AB} < 22$ mag. WAVES consists of two interlocking galaxy
surveys (WAVES-Deep and WAVES-Wide), providing the next two steps beyond the highly successful 1M galaxy Sloan Digital Sky Survey and the 250k Galaxy And Mass Assembly survey. WAVES will enable an unprecedented study of the distribution and evolution of mass, energy, and structures extending from 1-kpc dwarf galaxies in the local void to the morphologies of 200-Mpc filaments at $zsim1$. A key aim of both surveys will be to compare comprehensive empirical observations of the spatial properties of galaxies, groups, and filaments, against state-of-the-art numerical simulations to distinguish between various Dark Matter models.
We distribute an easy-to-use mock catalog of galaxies with detailed neutral atomic hydrogen (HI) and auxiliary molecular and optical properties. The catalog covers a field of 10-by-10 degrees and a redshift range of z=0-1.2. It contains galaxies with
21cm peak flux densities down to 1uJy and is, within this flux limit, complete for HI masses above 10^8 solar masses. Five random realisations of the catalog in ASCII format (~4GB/file) and subtables with HI flux limits of 10u Jy (~500MB/file) and 100uJy$ (~30MB/file) can be downloaded at http://ict.icrar.org/store/staff/do/s3sax.
Power-law relations between tracers of baryonic mass and rotational velocities of disk galaxies, so-called Tully-Fisher relations (TFRs), offer a wealth of applications in galaxy evolution and cosmology. However, measurements of rotational velocities
require galaxy inclinations, which are difficult to measure, thus limiting the range of TFR studies. This work introduces a maximum likelihood estimation (MLE) method for recovering the TFR in galaxy samples with limited or no information on inclinations. The robustness and accuracy of this method is demonstrated using virtual and real galaxy samples. Intriguingly, the MLE reliably recovers the TFR of all test samples, even without using any inclination measurements - that is, assuming a sin(i)-distribution for galaxy inclinations. Explicitly, this inclination-free MLE recovers the three TFR parameters (zero-point, slope, scatter) with statistical errors only about 1.5-times larger than the best estimates based on perfectly known galaxy inclinations with zero uncertainty. Thus, given realistic uncertainties, the inclination-free MLE is highly competitive. If inclination measurements have mean errors larger than 10 degrees, it is better not to use any inclinations, than to consider the inclination measurements to be exact. The inclination-free MLE opens interesting perspectives for future HI surveys by the SKA and its pathfinders.
