Improved Distances to Type Ia Supernovae with Multicolor Light-Curve Shapes: MLCS2k2

By S. Jha, A. Riess, R. Kirshner. 2006

599 citations recorded by the source corpus.

We present an updated version of the multicolor light-curve shape method to measure distances to Type Ia supernovae (SNe Ia), incorporating new procedures for K-correction and extinction corrections. We also develop a simple model to disentangle intrinsic color variations and reddening by dust and expand the method to incorporate U-band light curves and to more easily accommodate prior constraints on any of the model parameters. We apply this method to 133 nearby SNe Ia, including 95 objects in the Hubble flow (cz ≥ 2500 km s-1), which give an intrinsic dispersion of less than 7% in distance. The Hubble flow sample, which is of critical importance to all cosmological uses of SNe Ia, is the largest ever presented with homogeneous distances. We find that the Hubble flow SNe with H0dSN ≥ 7400 km s-1 yield an expansion rate that is 6.5% ± 1.8% lower than the rate determined from SNe within that distance, and this can have a large effect on measurements of the dark energy equation of state with SNe Ia. Peculiar velocities of SN Ia host galaxies in the rest frame of the Local Group are consistent with the dipole measured in the cosmic microwave background. Direct fits of SNe Ia that are significantly reddened by dust in their host galaxies suggest that their mean extinction law may be described by RV ≃ 2.7, but optical colors alone provide weak constraints on RV.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/160998cdee257d8e0825245cedaac3d6694cf375

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In Astronomy and Astrophysics

1. A. Riess
2. D. Schneider
3. Daniel J. Eisenstein
4. L. Hernquist
5. P. Hopkins
6. Simon D. M. White
7. A. Filippenko
8. J. Brinkmann

Citations in the corpus

• THE SLOAN DIGITAL SKY SURVEY-II SUPERNOVA SURVEY: SEARCH ALGORITHM AND FOLLOW-UP OBSERVATIONS (2007, background): “…the Calán/Tololo Supernova Search (Hamuy et al. 1993, 1996a,b,c) and by the CfA follow-up program (Riess et al. 1995; Riess 1996; Riess et al. 1999; Jha et al. 2006, 2007), and by studies pioneered by Pskovskii (1977) and by Phillips (1993) of the relationship between peak brightness and light…”
• Observational Constraints on the Nature of Dark Energy: First Cosmological Results from the ESSENCE Supernova Survey (2007, methodology): “Many variations on Phillips’ idea have been developed, including ∆m15 (Phillips et al. 1999), MLCS (Riess et al. 1996; Jha et al. 2007), DM15 (Prieto et al. 2006), stretch (Goldhaber et al. 2001), CMAGIC (Wang et al. 2003), and SALT (Guy et al. 2005).”
• SNLS3: CONSTRAINTS ON DARK ENERGY COMBINING THE SUPERNOVA LEGACY SURVEY THREE-YEAR DATA WITH OTHER PROBES (2011, methodology): “In particular, the MLCS2k2 fitter (Jha et al. 2007) has been widely used in previous SN Ia analyses (e.g. Hicken et al. 2009b; Kessler et al. 2009), and the use of MLCS2k2 versus SALT2 has led to significantly different cosmological parameters in some cases.”
• The Hubble series: convergence properties and redshift variables (2007, background): “µD and their estimated statistical uncertainties [7, 8, 9, 10, 11 ].”
• FIRST-YEAR SLOAN DIGITAL SKY SURVEY-II (SDSS-II) SUPERNOVA RESULTS: CONSTRAINTS ON NONSTANDARD COSMOLOGICAL MODELS (2009, methodology): “For the analysis presented in this paper we start by discussing the supernova dataset analyzed using the Multicolor Light Curve Shape 2k2 fitter: (MLCS; Jha et al. 2007)23.”
• A 2.4% DETERMINATION OF THE LOCAL VALUE OF THE HUBBLE CONSTANT (2016, methodology): “As an alternative to the SALT-II light-curve fitter, we used the MLCS2k2 fitter (Jha et al. 2007) with a value of RV=2.5 for the SN host galaxy, the same as the primary fits of R11.”
• Observational probes of cosmic acceleration (2012, result): “…the realization that the two main algorithms developed by other groups for global fitting of SN light curves and cosmological parameters — MLCS2k2 (Jha et al. 2007) and SALT2 (Guy et al. 2007) — initially gave statistically inconsistent cosmological results (w = −0.76± 0.07 vs. w = −0.96 ±…”
• A REDETERMINATION OF THE HUBBLE CONSTANT WITH THE HUBBLE SPACE TELESCOPE FROM A DIFFERENTIAL DISTANCE LADDER (2009, methodology): “Host SN Ia filters m0v,i + 5av σ a µ0,i − µ0,4258 NGC 4536 SN 1981B UBVR 15.156 0.145 1.145 (0.0845) NGC 4639 SN 1990N UBVRI 16.059 0.111 2.185 (0.0963) NGC 3982 SN 1998aq UBVRI 15.976 0.091 2.473 (0.101) NGC 3370 SN 1994ae UBVRI 16.578 0.102 2.831 (0.0771) NGC 3021 SN 1995al UBVRI 16.726 0.113 2.91”
• SEVEN-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE (WMAP) OBSERVATIONS: COSMOLOGICAL INTERPRETATION (2010, methodology): “We also found that the parameters of the minimal 6- parameter ΛCDM model derived from two compilations of Kessler et al. (2009) are different: one compilation uses the light curve fitter called SALT-II (Guy et al. 2007) while the other uses the light curve fitter called MLCS2K2 (Jha et al. 2007).”
• COSMICFLOWS-2: THE DATA (2013, methodology): “It has been amply demonstrated that SNIa events can be calibrated to acquire accurate distances (Phillips 1993; Jha et al. 2007; Hicken et al. 2009).”
• The dependence of Type Ia Supernovae luminosities on their host galaxies (2010, background): “Relations between the width of the SN Ia light curve and peak luminosity (Phillips 1993) and between the SN Ia optical colours and luminosity (e.g. Riess et al. 1996; Tripp 1998) reduce the scatter in their peak magnitudes to ∼0.15mag (Jha et al. 2007; Guy et al. 2007; Conley et al. 2008).”
• THE CARNEGIE SUPERNOVA PROJECT: LIGHT-CURVE FITTING WITH SNooPy (2010, methodology): “In this case, we use the prior from Jha et al. (2007), which corresponds to the convolution of a normal distribution N(0, σc) with an exponential tail exp(−E(B−V )/τ).”
• SUPERNOVA SIMULATIONS AND STRATEGIES FOR THE DARK ENERGY SURVEY (2011, methodology): “In this work, we use the optical (λ < 1 µm) MLCS2k2 (Jha et al. 2007) and SALT2 (Guy et al. 2007) models and the optical+infrared SNooPy model (Burns et al. 2011).”
• SPECTRA AND HUBBLE SPACE TELESCOPE LIGHT CURVES OF SIX TYPE Ia SUPERNOVAE AT 0.511 < z < 1.12 AND THE UNION2 COMPILATION (2010, methodology): “While the training of MLCS2k2 is exclusively based on observations of nearby SNe, the SiFTO and SALT2 training address this difficulty by also including high redshift data where the rest-frame U -band is observed at redder wavelengths.”
• PHOTOMETRIC SUPERNOVA CLASSIFICATION WITH MACHINE LEARNING (2016, methodology): “…we use existing supernova simulations from the Supernova Photometric Classification Challenge (SPCC) (Kessler et al. 2010a,b), which are simulated DES light curves built from an existing library of non-Ia templates and using both SALT2 (Guy et al. 2007) and MLCS2k2 (Jha et al. 2007) type Ia models.”