A lfa u ltra d eep s urvey
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Strategy: Very long integration time on small patches of sky. A LFA U ltra- D eep S urvey. Team leader: Wolfram Freudling. Team:

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A LFA U ltra- D eep S urvey

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A lfa u ltra d eep s urvey

Strategy: Very long integration time on small patches of sky

ALFA Ultra-Deep Survey

Team leader: Wolfram Freudling

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


A lfa u ltra d eep s urvey

Main Scientific Motivation: Evolution of gas content at z < 0.15

Evolution of star-formation rate

Extrapolation from Ly-α absorbers

STORRIE-LOMBARDI & WOLFE, 2000, ApJ 543, 552

PEI, FALL, & HAUSER 1999, ApJ, 522, 604

AUDS Survey


A lfa u ltra d eep s urvey

More Scientific Goals:

The Cosmic Web Low column-density gas in the local Universe Extragalactic OH Megamaser Emission Extragalactic HI Absorption

AUDS Survey


Possible survey parameters

Possible survey parameters

  • Need to be sensitive to MHI~109-10 M

  • 200 km/sec linewidth  0.2mJy at z~0.16

  • rms~0.05 mJy/beam (260x deeper than HIPASS)

  • 0.36 deg2 in 1000 hrs, or 70 hrs/beam

  • Volume = 8000 Mpc3

  • 160 galaxies in range 109-10 M

AUDS Survey


Precursor proposal to test sensitivity limitations on small region

Precursor Proposal to test sensitivity limitations on small region:

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  • σTint 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

AUDS Survey


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