The Supernova Legacy Survey: Measurement of Omega_M, Omega_Lambda,and w from the First Year Data Set

By P. Astier, J. Guy, N. Regnault, R. Pain, É. Aubourg, D. Balam, S. Basa, R. Carlberg, S. Fabbro, D. Fouchez and 32 more. 2005

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We present distance measurements to 71 high redshift type Ia supernovae discovered during the first year of the 5-year Supernova Legacy Survey (SNLS). These events were detected and their multi-color light-curves measured using the MegaPrime/MegaCam instrument at the Canada-France-Hawaii Telescope (CFHT), by repeatedly imaging four one-square degree fields in four bands. Follow-up spectroscopy was performed at the VLT, Gemini and Keck telescopes to confirm the nature of the supernovae and to measure their redshift. With this data set, we have built a Hubble diagram extending to z = 1, with all distance measurements involving at least two bands. Systematic uncertainties are evaluated making use of the multiband photometry obtained at CFHT. Cosmological fits to this first year SNLS Hubble diagram give the following results: {Omega}{sub M} = 0.263 {+-} 0.042 (stat) {+-} 0.032 (sys) for a flat {Lambda}CDM model; and w = -1.023 {+-} 0.090 (stat) {+-} 0.054 (sys) for a flat cosmology with constant equation of state w when combined with the constraint from the recent Sloan Digital Sky Survey measurement of baryon acoustic oscillations.

Subfields: Astronomy and Astrophysics, Instrumentation, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/43fa5bf57967d49fae38df556b9ebba811ad6226

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Citations in the corpus

The Pantheon+ Analysis: Cosmological Constraints (2022, methodology): “Constraining cosmological models with SN data using χ2 has been used in previous SN Ia cosmology analyses (e.g., Riess et al. 1998; Astier et al. 2006) and first included systematic covariance in Conley et al. (2011).”
The Complete Light-curve Sample of Spectroscopically Confirmed SNe Ia from Pan-STARRS1 and Cosmological Constraints from the Combined Pantheon Sample (2017, methodology): “The process also has many similarities to the method first presented in Astier et al. (2006), with recent updates in Astier et al. (2013).”
The Zwicky Transient Facility: System Overview, Performance, and First Results (2018, methodology): “…Survey (ASAS; Pojmanski 1997), the Lincoln Near-Earth Asteroid Research survey (LINEAR; Stokes et al. 2000), the Supernova Legacy Survey (SNLS; Astier et al. 2006), Palomar-Quest (Djorgovski et al. 2008), the Catalina Sky Survey (CSS; Larson et al. 2003) and associated Catalina Real-time…”
Low surface brightness galaxy rotation curves in the low energy limit of Rn gravity: no need for dark matter? (2006, background): “…(Eke et al. 1998; Viana et al. 2002; Bachall et al. 2003; Bachall & Bode 2003), the Hubble diagram of Type Ia Supernovae (Riess et al. 2004; Astier et al. 2006; Clocchiati et al. 2006), optical surveys of large scale structure (Pope et al. 2005; Cole et al. 2005; Eisenstein et al. 2005),…”
The WiggleZ Dark Energy Survey: survey design and first data release (2009, background): “…and the latest supernova data from the supernova legacy survey (SNLS), HST and Equation of State: Supernovae Trace Cosmic Expansion (ESSENCE) projects (Astier et al. 2006; Riess et al. 2007; Wood-Vasey et al. 2007) to predict marginalized errors in our model of σ ( m) = 0.02 and σ (wconst) = 0.07.”