1. ALFA Ultra-Deep Survey Team: Elias Brinks, Noah Brosch, Barbara Catinella, Christopher Conselice, Jonathan Davies, Erwin de Blok, Virginia Kilborn, Suzanne Linder, Karen Masters, Martin Meyer, Robert Minchin, Emmanuel Momjian, Karen O'Neil, Daniel Pisano, Jessica Rosenberg, Kristine Spekkens, Lister Staveley- Smith, Wim van Driel, Martin Zwaan Strategy: Very long integration time on small patches of sky Team leader: Wolfram Freudling

2. AUDS Survey2 STORRIE-LOMBARDI & WOLFE, 2000, ApJ 543, 552 PEI, FALL, & HAUSER 1999, ApJ, 522, 604 Main Scientific Motivation: Evolution of gas content at z < 0.15 Extrapolation from Ly-α absorbers Evolution of star-formation rate

3. AUDS Survey3 More Scientific Goals:  The Cosmic Web  Low column-density gas in the local Universe  Extragalactic OH Megamaser Emission  Extragalactic HI Absorption

4. AUDS Survey4 Possible survey parameters  Need to be sensitive to M HI ~10 9-10 M   200 km/sec linewidth  0.2mJy at z~0.16  rms~0.05 mJy/beam (260x deeper than HIPASS)  0.36 deg 2 in 1000 hrs, or 70 hrs/beam  Volume = 8000 Mpc 3  160 galaxies in range 10 9-10 M 

5. AUDS Survey5 Precursor Proposal to test sensitivity limitations on small region: ___  σ  T int for long integrations?  RFI  Baselines, standing waves  Efficiency (time on “source”) proposal: 70 hours of repeated drift scans over an area with known gas rich galaxies within 200Mhz bandpass