NOAO >   Observing Info >   Approved Programs >   2002B-0007

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Program Information for 2002B-0007


PI: Nicholas B Suntzeff, NOAO, nsuntzeff@tamu.edu
Address: CTIO, Casilla 603, La Serena CHILE

CoI: Brian Schmidt, Australia Telescope National Facility
CoI: Christopher Stubbs, U. of Washington
CoI: Robert P Kirshner, Harvard-Smithsonian Center for Astrophysics
CoI: Alexei V Filippenko, UC Berkeley
CoI: Peter Garnavich, U. of Notre Dame
CoI: Adam Riess, STScI
CoI: John L Tonry, U. of Hawaii
CoI: R Chris Smith, NOAO
CoI: Kevin Krisciunas, CTIO
CoI: Mark Phillips, Carnegie Institution of Washington
CoI: Alejandro Clocchiatti, Pontificia Universidad Catolica de Chile
CoI: Bruno Leibundgut, ESO
CoI: Jason Spyromilio, ESO
CoI: Brian Barris, U. of Hawaii
CoI: Weidong Li, UC Berkeley
CoI: Craig Hogan, U. of Washington
CoI: Gajus Miknaitis, U. of Washington
CoI: Steven Holland, U. of Notre Dame
CoI: Saurabh W Jha, Harvard-Smithsonian Center for Astrophysics
CoI: Thomas Matheson, Harvard-Smithsonian Center for Astrophysics
CoI: Jesper Sollerman, ESO
CoI: Peter Challis, Harvard-Smithsonian Center for Astrophysics
CoI: Steve Pompea, NOAO
CoI: Andrew Becker, Bell Labs, Lucent Technologies
CoI: Armin Rest, U. of Washington
CoI: Jason Quinn, U. of Notre Dame
CoI: Alberto Noriega-Crespo, IPAC

Title: The w Project: Measuring the Equation of State of the Universe

Abstract: We propose to find and follow $sim 200$ Type Ia supernovae with the Mosaic Imager on the Blanco 4-m telescope over a five-year period. This search is designed to find supernovae distributed evenly over the redshift range [0.15, 0.75]. The survey will obtain $VRI$ photometry which we will supplement with $zJ$ photometry and spectra using Keck, MMT, Magellan, Gemini, and the VLT. We aim to answer a simple, but very important, question: is the dark energy of the universe consistent with a cosmological constant ($w=-1$)? If not, this means the dark energy must be a more general energy field such as ``quintessence.\'\' This survey should determine $w$ to $pm.1 (1$sigma$). We propose to use the {it other} half of the 30 half-nights per year already assigned to the SuperMacho Team. We will exploit the {it same} data reduction pipelines already developed for SuperMacho to find SNe and to measure their light curves. By merging the two projects, we can use the same software, hardware, and people for two important investigations of matter and energy in the universe.

Program Type: Survey

Scheduled Nights:
Run 1 (2002B):  CT-4m/MOSAIC -- 15n on Sep 27 2002, Sep 29 2002, Oct 01 2002, Oct 03 2002, Oct 05 2002, Oct 07 2002, Oct 09 2002, Oct 11 2002, Oct 13 2002, Oct 29 2002, Oct 31 2002, Nov 02 2002, Nov 04 2002, Nov 06 2002, Nov 08 2002, Nov 10 2002, Nov 12 2002, Nov 14 2002, Nov 27 2002, Nov 29 2002, Dec 01 2002, Dec 03 2002, Dec 05 2002, Dec 07 2002, Dec 09 2002, Dec 11 2002, Dec 13 2002, Dec 15 2002, Dec 28 2002, Jan 02 2003
Run 1 (2003B):  CT-4m/MOSAIC -- 14.5n on Sep 27 2003, Oct 18 - Oct 19 2003, Oct 21 2003, Oct 23 2003, Oct 25 2003, Oct 27 2003, Oct 29 2003, Oct 31 2003, Nov 14 2003, Nov 16 2003, Nov 18 2003, Nov 20 2003, Nov 22 2003, Nov 24 2003, Nov 26 2003, Nov 28 2003, Nov 30 2003, Dec 02 2003, Dec 12 2003, Dec 14 2003, Dec 16 2003, Dec 18 2003, Dec 20 2003, Dec 22 2003, Dec 24 2003, Dec 26 2003, Dec 28 2003, Dec 30 2003
Run 1 (2004B):  CT-4m/MOSAIC -- 16n on Sep 17 2004, Sep 19 2004, Oct 04 2004, Oct 06 2004, Oct 08 2004, Oct 10 2004, Oct 12 2004, Oct 14 2004, Oct 16 2004, Oct 18 2004, Oct 20 2004, Oct 22 2004, Nov 03 2004, Nov 05 2004, Nov 07 2004, Nov 09 2004, Nov 11 2004, Nov 13 2004, Nov 15 2004, Nov 17 2004, Nov 19 2004, Nov 21 2004, Dec 02 2004, Dec 04 2004, Dec 06 2004, Dec 08 2004, Dec 10 2004, Dec 12 2004, Dec 14 2004, Dec 16 2004, Dec 18 2004, Dec 20 2004
Run 1 (2005B):  CT-4m/MOSAIC -- 15n on Sep 23 2005, Sep 25 2005, Sep 27 2005, Sep 29 2005, Oct 01 2005, Oct 03 2005, Oct 05 2005, Oct 08 2005, Oct 10 2005, Oct 24 2005, Oct 26 2005, Oct 28 2005, Oct 30 2005, Nov 01 2005, Nov 03 2005, Nov 05 2005, Nov 07 2005, Nov 09 2005, Nov 21 2005, Nov 23 2005, Nov 25 2005, Nov 27 2005, Nov 29 2005, Dec 01 2005, Dec 03 2005, Dec 07 2005, Dec 09 2005, Dec 26 2005, Dec 30 2005, Jan 05 2006
Run 1 (2006B):  CT-4m/MOSAIC -- 15n on Sep 15 2006, Sep 18 2006, Sep 21 2006, Sep 24 2006, Sep 27 2006, Oct 12 2006, Oct 14 2006, Oct 16 2006, Oct 18 2006, Oct 20 2006, Oct 22 2006, Oct 24 2006, Oct 26 2006, Oct 28 2006, Oct 30 2006, Nov 11 2006, Nov 13 2006, Nov 15 2006, Nov 17 2006, Nov 19 2006, Nov 21 2006, Nov 23 2006, Nov 25 2006, Nov 27 2006, Nov 29 2006, Dec 12 2006, Dec 14 2006, Dec 16 2006, Dec 18 2006, Dec 20 2006
Run 1 (2007B):  CT-4m/MOSAIC -- 15n on Oct 01 2007, Oct 03 2007, Oct 05 2007, Oct 07 2007, Oct 09 2007, Oct 11 2007, Oct 13 2007, Oct 15 2007, Oct 17 2007, Oct 19 2007, Oct 31 2007, Nov 02 2007, Nov 04 2007, Nov 06 2007, Nov 08 2007, Nov 10 2007, Nov 12 2007, Nov 14 2007, Nov 16 2007, Nov 18 2007, Nov 30 2007, Dec 02 2007, Dec 04 2007, Dec 06 2007, Dec 08 2007, Dec 10 2007, Dec 12 2007, Dec 14 2007, Dec 16 2007, Dec 18 2007
Run 2 (2002B):  CT-1.5m/CFIM -- 12n on Nov 05 - Nov 08 2002, Dec 01 - Dec 04 2002, Jan 28 - Jan 31 2003
Run 3 (2002B):  WIYN/MIMO -- 4n on Oct 26 2002, Nov 16 2002, Dec 04 2002, Jan 28 2003
Run 3 (2003B):  WIYN/MIMO -- 4n on Nov 15 2003, Dec 23 2003, Jan 08 2004, Jan 12 2004
Run 3 (2004B):  WIYN/MIMO -- 4n on Dec 02 2004, Dec 17 2004, Jan 04 2005, Jan 09 2005
Run 3 (2005B):  WIYN/MIMO -- 4n on Oct 12 2005, Nov 26 2005, Dec 06 2005, Jan 16 2006
Run 3 (2006B):  WIYN/MIMO -- 4n on Sep 17 2006, Oct 31 2006, Dec 11 2006, Jan 23 2007
Run 4 (2003B):  CT-0.9m/CFIM -- 14n on Nov 18 - Nov 24 2003, Dec 23 - Dec 29 2003
Run 4 (2004B):  CT-0.9m/CFIM -- 15n on Nov 09 - Nov 15 2004, Jan 03 - Jan 10 2005
Run 4 (2005B):  CT-0.9m/CFIM -- 15n on Oct 25 - Oct 31 2005, Nov 25 - Nov 30 2005, Dec 22 - Dec 23 2005
Run 4 (2006B):  CT-0.9m/CFIM -- 4n on Nov 23 2006, Dec 21 - Dec 23 2006
Run 4 (2007B):  CT-0.9m/CFIM -- 4n on Dec 20 - Dec 23 2007
Run 5 (2006B):  CT-0.9m-SVC/CFIM -- 55hrs
Run 5 (2007B):  CT-0.9m-SVC/CFIM -- 100hrs


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