The Supernova Legacy Survey 3-year sample: Type Ia supernovae photometric distances and cosmological constraints ,

By J. Guy, M. Sullivan, A. Conley, N. Regnault, P. Astier, C. Balland, S. Basa, R. Carlberg, D. Fouchez, D. Hardin and 24 more. 2010

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Aims. We present photometric properties and distance measurements of 252 high redshift Type Ia supernovae (0.15 < z < 1.1) discovered during the first three years of the Supernova Legacy Survey (SNLS). These events were detected and their multi-colour 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 redshifts. Methods. Systematic uncertainties arising from light curve modeling are studied, making use of two techniques to derive the peak magnitude, shape and colour of the supernovae, and taking advantage of a precise calibration of the SNLS fields. Results. A flat ΛCDM cosmological fit to 231 SNLS high redshift type Ia supernovae alone gives Ω_M = 0.211 ± 0.034(stat) ± 0.069(sys). The dominant systematic uncertainty comes from uncertainties in the photometric calibration. Systematic uncertainties from light curve fitters come next with a total contribution of ± 0.026 on Ω_M. No clear evidence is found for a possible evolution of the slope (β) of the colour-luminosity relation with redshift.

Subfields: Astronomy and Astrophysics

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THE HUBBLE SPACE TELESCOPE CLUSTER SUPERNOVA SURVEY. V. IMPROVING THE DARK-ENERGY CONSTRAINTS ABOVE z > 1 AND BUILDING AN EARLY-TYPE-HOSTED SUPERNOVA SAMPLE (2011, background): “While some individual sets of SNe Ia are now, by themselves, large enough to provide constraints on some cosmological parameters (Guy et al. 2010; Kessler et al. 2009), they do not yet constrain the properties of dark energy as well as analyses that combine individual data-sets to create a…”
A Comprehensive Measurement of the Local Value of the Hubble Constant with 1 km s−1 Mpc−1 Uncertainty from the Hubble Space Telescope and the SH0ES Team (2021, methodology): “It is a simpler description, where the intrinsic scatter of SNe Ia is monochromatic (i.e., dispersion only in the luminosity, not the color) from Guy et al. (2010) and used in the JLA analysis (Betoule et al. 2014) and in the first Pantheon compilation (Scolnic et al. 2018).”
Clarifying the Hubble constant tension with a Bayesian hierarchical model of the local distance ladder (2017, methodology): “The Hubble flow SNe are sourced from catalogues compiled by Riess et al. (1999); Jha et al. (2006); Hicken et al. (2009, 2012); Guy et al. (2010); Stritzinger et al. (2011); Rest et al. (2014) and Sako et al. (2014), and calibrated according to Scolnic et al. (2015) and Scolnic & Kessler (2016)7.”
Spectrophotometric time series of SN 2011fe from the Nearby Supernova Factory (2013, background): “SNe Ia have since become a key means for constraining the unknown physics of cosmic acceleration, called “Dark Energy” (e.g., Guy et al. 2010; Howell 2011; Suzuki et al. 2012).”
TYPE Ia SUPERNOVA RATE MEASUREMENTS TO REDSHIFT 2.5 FROM CANDELS: SEARCHING FOR PROMPT EXPLOSIONS IN THE EARLY UNIVERSE (2014, methodology): “We again use SNANA as our simulation engine, this time generating 100,000 SN Ia based on the SALT2 light curve model (Guy et al. 2010).”
Improved cosmological constraints from a joint analysis of the SDSS-II and SNLS supernova samples (2014, methodology): “Otherwise, we follow closely the approach described in the analysis of the first three years of SNLS (Guy et al. 2010; Conley et al. 2011; Sullivan et al. 2011).”
On the Hubble Constant Tension in the SNe Ia Pantheon Sample (2021, unknown): “Since, in principle, there are no reasons to prefer one model over the other, the average of G10 and C11 bias corrections is taken, and this constitutes the systematic part of the covariance matrix, denoted as Csys (Scolnic et al. 2018).”
The Intrinsic Alignment of Galaxies and its Impact on Weak Gravitational Lensing in an Era of Precision Cosmology (2014, background): “…2012; Blake et al., 2012; Padmanabhan et al., 2012), constraints on H0 (Riess et al., 2011; Freedman et al., 2012), type Ia supernovae (SNe Ia) (Guy et al., 2010; Conley et al., 2011; Sullivan et al., 2011; Suzuki et al., 2012), and weak gravitational lensing (Bacon et al., 2000; van Waerbeke…”
Correcting Type Ia Supernova Distances for Selection Biases and Contamination in Photometrically Identified Samples (2016, methodology): “The SALT-II framework (Guy et al. 2010) is used for light curve fitting, and a nearest neighbor (NN) method is used for photometric classification.”
CFHTLenS: the Canada–France–Hawaii Telescope Lensing Survey – imaging data and catalogue products (2012, background): “Note that the width of the CFHT i′-band filter is sufficiently narrow that we can assume the PSF is independent of the star colour (Cypriano et al. 2010; Voigt et al. 2012), which is shown to be a good assumption for the i′-band in Guy et al. (2010).”
REDDENING AND EXTINCTION TOWARD THE GALACTIC BULGE FROM OGLE-III: THE INNER MILKY WAY'S RV ∼ 2.5 EXTINCTION CURVE (2012, methodology): “We note that studies of the extinction in the hosts of type Ia SNe routinely find an RV ≈ 2.5 extinction curve (Guy et al. 2010; Chotard et al. 2011; Mandel et al. 2011), and then subsequently assume the functional dependence on wavelength calibrated in investigations of Milky Way extinction.”
On the Evolution of the Hubble Constant with the SNe Ia Pantheon Sample and Baryon Acoustic Oscillations: A Feasibility Study for GRB-Cosmology in 2030 (2022, methodology): “Considering the color and stretch population models for SNe Ia, in our approach we average the distance moduli given by the [206] (G2010) and [207] (C2011) models.”
SNLS3: CONSTRAINTS ON DARK ENERGY COMBINING THE SUPERNOVA LEGACY SURVEY THREE-YEAR DATA WITH OTHER PROBES (2011, methodology): “Fortunately this is a tractable problem as the uncertainties are understood in modern SN Ia samples and can be accurately modeled, albeit only after detailed and painstaking work (Regnault et al. 2009; Guy et al. 2010; Conley et al. 2011).”
The WiggleZ Dark Energy Survey: the growth rate of cosmic structure since redshift z=0.9 (2011, methodology): “In addition to providing a good description of the temperature and polarization fluctuations in the CMB, this model yields a good fit to distance measurements from supernovae and baryon acoustic oscillations (Guy et al. 2010, Percival et al. 2010).”
Completed SDSS-IV extended Baryon Oscillation Spectroscopic Survey: Cosmological implications from two decades of spectroscopic surveys at the Apache Point Observatory (2020, methodology): “…and analysis methodology (Jha et al. 2006; Riess et al. 2007; Frieman et al. 2008; Dawson et al. 2009; Hicken et al. 2009; Contreras et al. 2010; Guy et al. 2010; Conley et al. 2011; Sullivan et al. 2011), and direct measurements of the local expansion rate using Cepheid variables and SNe Ia…”
The Complete Light-curve Sample of Spectroscopically Confirmed SNe Ia from Pan-STARRS1 and Cosmological Constraints from the Combined Pantheon Sample (2017, methodology): “While multiple light-curve fitters can be used to determine accurate distances (e.g., Jha et al. 2007; Guy et al. 2010; Burns et al. 2011; Mandel et al. 2011), we use SALT2 (Guy et al. 2010) for this analysis, as it has been trained on the JLA sample (B14) and it is easy to assess various…”