FIRST-YEAR SLOAN DIGITAL SKY SURVEY-II SUPERNOVA RESULTS: HUBBLE DIAGRAM AND COSMOLOGICAL PARAMETERS

By R. Kessler, A. Becker, D. Cinabro, J. Vanderplas, J. Frieman, J. Marriner, T. Davis, B. Dilday, J. Holtzman, S. Jha and 36 more. 2009

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We present measurements of the Hubble diagram for 103 Type Ia supernovae (SNe) with redshifts 0.04 < z < 0.42, discovered during the first season (Fall 2005) of the Sloan Digital Sky Survey-II (SDSS-II) Supernova Survey. These data fill in the redshift “desert” between low- and high-redshift SN Ia surveys. Within the framework of the mlcs2k2 light-curve fitting method, we use the SDSS-II SN sample to infer the mean reddening parameter for host galaxies, RV = 2.18 ± 0.14stat ± 0.48syst, and find that the intrinsic distribution of host-galaxy extinction is well fitted by an exponential function, P(AV) = exp(−AV/τV), with τV = 0.334 ± 0.088 mag. We combine the SDSS-II measurements with new distance estimates for published SN data from the ESSENCE survey, the Supernova Legacy Survey (SNLS), the Hubble Space Telescope (HST), and a compilation of Nearby SN Ia measurements. A new feature in our analysis is the use of detailed Monte Carlo simulations of all surveys to account for selection biases, including those from spectroscopic targeting. Combining the SN Hubble diagram with measurements of baryon acoustic oscillations from the SDSS Luminous Red Galaxy sample and with cosmic microwave background temperature anisotropy measurements from the Wilkinson Microwave Anisotropy Probe, we estimate the cosmological parameters w and ΩM, assuming a spatially flat cosmological model (FwCDM) with constant dark energy equation of state parameter, w. We also consider constraints upon ΩM and ΩΛ for a cosmological constant model (ΛCDM) with w = −1 and non-zero spatial curvature. For the FwCDM model and the combined sample of 288 SNe Ia, we find w = −0.76 ± 0.07(stat) ± 0.11(syst), ΩM = 0.307 ± 0.019(stat) ± 0.023(syst) using mlcs2k2 and w = −0.96 ± 0.06(stat) ± 0.12(syst), ΩM = 0.265 ± 0.016(stat) ± 0.025(syst) using the salt-ii fitter. We trace the discrepancy between these results to a difference in the rest-frame UV model combined with a different luminosity correction from color variations; these differences mostly affect the distance estimates for the SNLS and HST SNe. We present detailed discussions of systematic errors for both light-curve methods and find that they both show data-model discrepancies in rest-frame U band. For the salt-ii approach, we also see strong evidence for redshift-dependence of the color-luminosity parameter (β). Restricting the analysis to the 136 SNe Ia in the Nearby+SDSS-II samples, we find much better agreement between the two analysis methods but with larger uncertainties: w = −0.92 ± 0.13(stat)+0.10−0.33(syst) for mlcs2k2 and w = −0.92 ± 0.11(stat)+0.07−0.15 (syst) for salt-ii.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

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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…”
Hubble Space Telescope spectra of the type Ia supernova SN 2011fe: a tail of low-density, high-velocity material with Z < Z⊙ (2013, background): “Type Ia supernovae (SNe Ia) remain a well-exploited cosmological probe and an immediate route to understanding the nature of dark energy (e.g. Riess et al. 1998; Perlmutter et al. 1999; Riesset al. ⋆ E-mail: P.Mazzali@ljmu.ac.uk 2007; Kessler et al. 2009; Sullivan et al. 2011; Suzuki et al.2012).”
TYPE Ia SUPERNOVA LIGHT CURVE INFERENCE: HIERARCHICAL MODELS IN THE OPTICAL AND NEAR-INFRARED (2010, methodology): “Kessler et al. (2009) found that differences in the U-band model between MLCS2k2 and SALT2 lead to large (Δw ∼ 0.2) differences in the cosmology using high-redshift samples.”
The VISTA deep extragalactic observations (VIDEO) survey (2012, background): “There are several outstanding challenges to progress in Type Ia supernova (SN Ia) cosmology (Conley et al. 2007; Kessler et al. 2009; Conley et al. 2011).”
The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: Constraining modified gravity (2016, methodology): “…analysis (JLA) of SN Ia observations by Betoule et al. (2014), a compilation of 740 SN Ia from the SDSS-II supernovae survey (Frieman et al. 2008; Kessler et al. 2009; Sollerman et al. 2009; Lampeitl et al. 2009; Campbell et al. 2013) as well as the Supernova Legacy Survey (SNLS, Astier et al.…”
TYPE Ia SUPERNOVA RATE MEASUREMENTS TO REDSHIFT 2.5 FROM CANDELS: SEARCHING FOR PROMPT EXPLOSIONS IN THE EARLY UNIVERSE (2014, methodology): “The mid-dust model is equivalent to the exponential distribution of Kessler et al. (2009a): P (AV ) = e −AV /τ , with τ = 0.33.”
Constraining primordial non-Gaussianity with future galaxy surveys (2011, positive): “For example the Sloan Digital Sky Survey (SDSS) (Aihara et al. 2011) and its follow-ups have greatly improved our understanding of the standard model, especially thanks to the measurement of galaxy clustering and baryon acoustic oscillations (see e.g. Percival et al. 2007), but also using galaxy clu”
Early-time light curves of Type Ib/c supernovae from the SDSS-II Supernova Survey (2014, methodology): “Results based on the first season of SN Ia data were presented in Kessler et al. (2009); Sollerman et al. (2009); Lampeitl et al. (2010), while Betoule et al. (2014) make use of the intermediate redshift (0.05< z <0.4) SN Ia data collected during all the three SDSS-II seasons.”
The Complete Light-curve Sample of Spectroscopically Confirmed SNe Ia from Pan-STARRS1 and Cosmological Constraints from the Combined Pantheon Sample (2017, methodology): “…(Contreras et al. 2010; Folatelli et al. 2010; Stritzinger et al. 2011), SNLS (Conley et al. 2011; Sullivan et al. 2011), SDSS (Frieman et al. 2008; Kessler et al. 2009a), and high-z data (z>1.0) from the SCP survey (Suzuki et al. 2012), GOODS (Riess et al. 2007), and CANDELS/ CLASH survey (Graur…”
THE EFFECT OF HOST GALAXIES ON TYPE Ia SUPERNOVAE IN THE SDSS-II SUPERNOVA SURVEY (2010, methodology): “We follow the procedure of Kessler et al. (2009a) and remove any object with a low probability of being a SN Ia (i.e. those with P (Ia) < 10−3), or which has an unphysical value of ∆ < −0.4.”
THE CARNEGIE SUPERNOVA PROJECT: LIGHT-CURVE FITTING WITH SNooPy (2010, background): “…of LSN ≃ 1043erg · s−1, SN Ia can be observed from the ground and space out to cosmological distances, thereby constraining the expansion history of the Universe (Freedman et al. 2009; Kessler et al. 2009; Wood-Vasey et al. 2007; Astier et al. 2006; Perlmutter et al. 1999; Riess et al. 1998).”
GALAXY CLUSTERING IN THE COMPLETED SDSS REDSHIFT SURVEY: THE DEPENDENCE ON COLOR AND LUMINOSITY (2010, background): “…baryon density parameter Ωb = 0.045, consistent with recent determinations from the cosmic microwave background (WMAP5; Hinshaw et al. 2009; Dunkley et al. 2009; Komatsu et al. 2009), supernova Ia (Kowalski et al. 2008; Kessler et al. 2009), and baryon acoustic oscillations (Percival et al. 2010).”
The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: measurements of the growth of structure and expansion rate at z = 0.57 from anisotropic clustering (2012, methodology): “1 I N T RO D U C T I O N Measurements of the cosmic distance–redshift relation using supernovae (Riess et al. 1998; Perlmutter et al. 1999; Kessler et al. 2009; Amanullah et al. 2010), the cosmic microwave background (CMB; Ade et al. 2011; Larson et al. 2011), the local expansion rate (Riess et al.…”
THE BARYON OSCILLATION SPECTROSCOPIC SURVEY OF SDSS-III (2012, background): “Host Galaxies of SDSS-II SNe: While many SNe Ia identified in the SDSS-II program (Frieman et al. 2008) were spectroscopically confirmed and used in the first year cosmology results (Kessler et al. 2009), most SNe and their host galaxies have not been observed spectroscopically.”
The dependence of Type Ia Supernovae luminosities on their host galaxies (2010, background): “Such an evolution has been claimed (Kessler et al. 2009), though is not present to any significant extent in SNLS3 data (Guy et al. 2010).”
SPECTRA AND HUBBLE SPACE TELESCOPE LIGHT CURVES OF SIX TYPE Ia SUPERNOVAE AT 0.511 < z < 1.12 AND THE UNION2 COMPILATION (2010, background): “…(hereafter H09) added a significant number of nearby SNe to a subset of the “Union” set to create a new compilation, and similarly the SDSS SN survey (Kessler et al. 2009) (hereafter KS09) carried out an analysis of a compilation including their large intermediate-z data set (Holtzman et al. 2008).”