NOAO >   Observing Info >   Approved Programs >   1999B-0018

Small NOAO Logo

Program Information for 1999B-0018


PI: J Anthony Tyson, Bell Labs, Lucent Technologies, tyson@physics.ucdavis.edu
Address: 700 Mountain Ave., Murray Hill, NJ 07974 USA

CoI: Gary Bernstein, U. of Michigan
CoI: Ian dell'Antonio, Brown U.
CoI: David Wittman, Bell Labs, Lucent Technologies
CoI: David Kirkman, Bell Labs, Lucent Technologies
CoI: Greg Kochanski, Bell Labs, Lucent Technologies
CoI: Tod R Lauer, NOAO
CoI: Thomas Broadhurst, UC Berkeley
CoI: Renyue Cen, Princeton U.
CoI: Judith G Cohen, California Institute of Technology
CoI: Anthony H Gonzalez, UC Santa Cruz
CoI: Puragra Guhathakurta, UC Santa Cruz
CoI: Wayne Hu, Institute for Advanced Study
CoI: Nick Kaiser, U. of Hawaii
CoI: Jordi Miralda-Escude, U. of Pennsylvania
CoI: David N Spergel, Princeton U.
CoI: Gordon Squires, California Institute of Technology
CoI: Christopher Stubbs, U. of Washington
CoI: Andrew Becker, U. of Washington
CoI: Hossein Khiabanian, Brown U.
CoI: Robert A Schommer, CTIO
CoI: Donald Sweeney, U. of Arizona

Title: Deep Lens Survey

Abstract: This Survey will produce the first unbiased maps of the large-scale structure of the mass distribution beyond the local Universe. We will obtain very deep multicolor imaging of seven 2$^circ$ fields, which we will use to measure the shear of distant galaxies induced by the mass of foreground structures. These weak-lensing observations are sensitive to all forms of clumped mass and will yield unbiased mass maps with resolution of 1arcmin in the plane of the sky ($sim 120$ $h^$ kpc at $z = 0.2$), in multiple redshift ranges (with $Delta z = 0.5 z$). These maps will measure for the first time the change in large scale structure from z=1 to the present epoch, and test the current theories of structure formation, which predict that mass in the low-redshift Universe has a particular filamentary/sheetlike structure. These unique observations will constrain the clustering properties of matter, most notably $Omega_{rm matter}$ and $Omega_Lambda$, and, when compared with the results from microwave background anisotropy missions, will test the basic theory of structure formation via gravitational instability.

Program Type: Survey

Scheduled Nights:
Run 1 (1999B):  KP-4m/MOSA -- 3.5n on Nov 08 - Nov 10 1999, Dec 11 - Dec 14 1999
Run 1 (2000B):  KP-4m/MOSA -- 5.5n on Nov 22 - Nov 26 2000, Dec 18 - Dec 23 2000
Run 1 (2001B):  KP-4m/MOSA -- 6n on Nov 13 - Nov 18 2001, Dec 14 - Dec 19 2001
Run 1 (2002A):  KP-4m/MOSA -- 2n on Apr 09 - Apr 12 2002
Run 1 (2002B):  KP-4m/MOSA -- 10.5n on Nov 27 - Dec 02 2002, Jan 03 - Jan 08 2003
Run 1 (2003A):  KP-4m/MOSA -- 4n on Mar 06 - Mar 09 2003
Run 1 (2003B):  KP-4m/MOSA -- 6n on Oct 27 - Nov 01 2003
Run 1 (2004A):  KP-4m/MOSA -- 2.5n on Mar 24 - Mar 28 2004
Run 2 (2000A):  CT-4m/MOSAIC -- 6n on Mar 03 - Mar 08 2000, Apr 01 - Apr 06 2000
Run 2 (2000B):  CT-4m/MOSAIC -- 2n on Jan 22 - Jan 25 2001
Run 2 (2001A):  CT-4m/MOSAIC -- 4n on Feb 23 - Feb 26 2001, Mar 23 - Mar 26 2001
Run 2 (2001B):  CT-4m/MOSAIC -- 2.5n on Jan 09 - Jan 12 2002, Jan 14 2002
Run 2 (2002A):  CT-4m/MOSAIC -- 5.5n on Feb 13 - Feb 18 2002, Apr 09 - Apr 13 2002
Run 2 (2002B):  CT-4m/MOSAIC -- 4n on Sep 05 - Sep 08 2002
Run 2 (2003A):  CT-4m/MOSAIC -- 14n on Feb 27 - Mar 05 2003, Mar 30 - Apr 05 2003
Run 2 (2003B):  CT-4m/MOSAIC -- 6n on Jan 15 - Jan 20 2004
Run 2 (2004A):  CT-4m/MOSAIC -- 6n on Mar 18 - Mar 23 2004


National Optical Astronomy Observatory, 950 North Cherry Avenue, P.O. Box 26732, Tucson, Arizona 85726, Phone: (520) 318-8000, Fax: (520) 318-8360



NOAO >   Observing Info >   Approved Programs >   1999B-0018

noaoprop-help@noao.edu

Small NOAO Logo