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Title:
The ESSENCE Supernova Survey: Survey Optimization, Observations, and Supernova Photometry
Authors:
Miknaitis, G.; Pignata, G.; Rest, A.; Wood-Vasey, W. M.; Blondin, S.; Challis, P.; Smith, R. C.; Stubbs, C. W.; Suntzeff, N. B.; Foley, R. J.; Matheson, T.; Tonry, J. L.; Aguilera, C.; Blackman, J. W.; Becker, A. C.; Clocchiatti, A.; Covarrubias, R.; Davis, T. M.; Filippenko, A. V.; Garg, A.; Garnavich, P. M.; Hicken, M.; Jha, S.; Krisciunas, K.; Kirshner, R. P.; Leibundgut, B.; Li, W.; Miceli, A.; Narayan, G.; Prieto, J. L.; Riess, A. G.; Salvo, M. E.; Schmidt, B. P.; Sollerman, J.; Spyromilio, J.; Zenteno, A.
Affiliation:
AA(Fermi National Accelerator Laboratory, Batavia, IL 60510-0500 .), AB(Pontificia Universidad Católica de Chile, Departamento de Astronomía y Astrofísica, Casilla 306, Santiago 22, Chile.), AC(Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, Casilla 603, La Serena, Chile.), AD(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138.), AE(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138.), AF(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138.), AG(Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, Casilla 603, La Serena, Chile.), AH(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138.; Department of Physics, Harvard University, Cambridge, MA 02138.), AI(Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, Casilla 603, La Serena, Chile.; Department of Physics, Texas A&M University, College Station, TX 77843-4242.), AJ(Department of Astronomy, University of California, Berkeley, CA 94720-3411.), AK(National Optical Astronomy Observatory, Tucson, AZ 85719-4933.), AL(Institute for Astronomy, University of Hawaii, Honolulu, HI 96822.), AM(Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, Casilla 603, La Serena, Chile.), AN(Research School of Astronomy and Astrophysics, Australian National University, Mount Stromlo and Siding Spring Observatories, Weston Creek PO 2611, Australia.), AO(Department of Astronomy, University of Washington, Seattle, WA 98195-1580.), AP(Pontificia Universidad Católica de Chile, Departamento de Astronomía y Astrofísica, Casilla 306, Santiago 22, Chile.), AQ(Department of Astronomy, University of Washington, Seattle, WA 98195-1580.), AR(Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, DK-2100 Copenhagen, Denmark.), AS(Department of Astronomy, University of California, Berkeley, CA 94720-3411.), AT(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138.; Department of Physics, Harvard University, Cambridge, MA 02138.), AU(Department of Physics, University of Notre Dame, Notre Dame, IN 46556-5670.), AV(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138.; Department of Physics, Harvard University, Cambridge, MA 02138.), AW(Department of Astronomy, University of California, Berkeley, CA 94720-3411.; Kavli Institute for Particle Astrophysics and Cosmology, Stanford Linear Accelerator Center, MS 29, Menlo Park, CA 94025.), AX(Department of Physics, Texas A&M University, College Station, TX 77843-4242.; Department of Physics, University of Notre Dame, Notre Dame, IN 46556-5670.), AY(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138.), AZ(European Southern Observatory, D-85748 Garching, Germany.), BA(Department of Astronomy, University of California, Berkeley, CA 94720-3411.), BB(Department of Astronomy, University of Washington, Seattle, WA 98195-1580.), BC(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138.; Department of Physics, Harvard University, Cambridge, MA 02138.), BD(Department of Astronomy, Ohio State University, Columbus, OH 43210.), BE(Space Telescope Science Institute, Baltimore, MD 21218.; Johns Hopkins University, Baltimore, MD 21218.), BF(Research School of Astronomy and Astrophysics, Australian National University, Mount Stromlo and Siding Spring Observatories, Weston Creek PO 2611, Australia.), BG(Research School of Astronomy and Astrophysics, Australian National University, Mount Stromlo and Siding Spring Observatories, Weston Creek PO 2611, Australia.), BH(Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, DK-2100 Copenhagen, Denmark.; Department of Astronomy, Stockholm University, AlbaNova, 10691 Stockholm, Sweden.), BI(European Southern Observatory, D-85748 Garching, Germany.), BJ(Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, Casilla 603, La Serena, Chile.)
Publication:
The Astrophysical Journal, Volume 666, Issue 2, pp. 674-693. (ApJ Homepage)
Publication Date:
09/2007
Origin:
UCP
ApJ Keywords:
Cosmology: Observations, Methods: Data Analysis, Stars: Supernovae: General, Surveys
DOI:
10.1086/519986
Bibliographic Code:
2007ApJ...666..674M

Abstract

We describe the implementation and optimization of the ESSENCE supernova survey, which we have undertaken to measure the dark energy equation-of-state parameter, w=P/(ρc2). We present a method for optimizing the survey exposure times and cadence to maximize our sensitivity to w for a given fixed amount of telescope time. For our survey on the CTIO 4 m telescope, measuring the luminosity distances and redshifts for supernovae at modest redshifts (z~0.5+/-0.2) is optimal for determining w. We describe the data analysis pipeline based on using reliable and robust image subtraction to find supernovae automatically and in nearly real time. Since making cosmological inferences with supernovae relies crucially on accurate measurement of their apparent brightnesses, we describe our efforts to establish a thorough calibration of the CTIO 4 m telescope's natural photometric system. In its first four years, ESSENCE has discovered and spectroscopically confirmed 102 Type Ia supernovae, at redshifts from 0.10 to 0.78, identified through an impartial, effective methodology for spectroscopic classification and redshift determination. We present the resulting light curves for all of the Type Ia supernovae found by ESSENCE and used in our measurement of w, presented in a companion paper by Wood-Vasey and coworkers.
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