SALT : a spectral adaptive light curve template for type Ia supernovae

By J. Guy, P. Astier, S. Nobili, N. Regnault, R. Pain. 2005

246 citations recorded by the source corpus.

We present a new method to parameterize type Ia Supernovae (SN Ia) multi-color light curves. The method was developed in order to analyze the large number of SN Ia multi-color light curves measured in current high-redshift projects. The technique is based on empirically modeling SN Ia luminosity variations as a function of phase, wavelength, a shape parameter, and a color parameter. The model is trained with a sample of well-measured nearby SN Ia and then tested with an independent set of supernovae by building an optimal luminosity distance estimator that combines the supernova rest-frame luminosity, shape parameter, and color reconstructed with the model. The distances we measure using B - and V -band data show a dispersion around the Hubble line comparable or lower than obtained with other methods. With this model, we are able to measure distances using  U - and B -band data with a dispersion of $0.16\pm0.05$ around the Hubble line.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/1040b32fc4b12507c488620460bf67acedbbe6b3

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In Astronomy and Astrophysics

1. A. Riess
2. A. Filippenko
3. D. Schneider
4. L. Hernquist
5. P. Hopkins
6. Daniel J. Eisenstein
7. R. Kirshner
8. S. Jha

Citations in the corpus

• The Carnegie Supernova Project: Absolute Calibration and the Hubble Constant (2018, background): “D, Santiago, Chile 9 Deceased 10 Cerro Tololo Inter-American Observatory, Casilla 603, La Serena, Chile 11 SOAR Telescope, Casilla 603, La Serena, Chile rameter ∆ (Riess et al. 1996; Jha et al. 2007), and the Spectral Adaptive Light curve Template (SALT) stretchlike parameter x1 (Guy et al. 2005).”
• A REDETERMINATION OF THE HUBBLE CONSTANT WITH THE HUBBLE SPACE TELESCOPE FROM A DIFFERENTIAL DISTANCE LADDER (2009, methodology): “We also changed the algorithm used to fit and compare the SN Ia light and color curves from MLCS2k2 to the SALT II (Guy et al. 2005) approach.”
• THE CARNEGIE SUPERNOVA PROJECT: ANALYSIS OF THE FIRST SAMPLE OF LOW-REDSHIFT TYPE-Ia SUPERNOVAE (2009, methodology): “This formalism was originally employed by Tripp & Branch (1999) to derive cosmological parameters from SN Ia data, and is part of the SALT (Guy et al. 2005) method used by Astier et al. (2006).”
• New Hubble Space Telescope Discoveries of Type Ia Supernovae at z ≥ 1: Narrowing Constraints on the Early Behavior of Dark Energy (2006, methodology): “Analyses that seek to correlate SN color with luminosity, such as those by Tripp & Branch (1999), Guy et al. (2005), and Astier et al. (2006), combine both the reddening-law parameter RV and intrinsic luminosity-color relation parameter into a single relation.”
• SALT2: using distant supernovae to improve the use of type Ia supernovae as distance indicators (2007, methodology): “In Guy et al. (2005) (hereafter SALT), we have applied broadband corrections to the spectral sequence N02 as a function of phase, wavelength and a stretch factor so that the spectra integrated in response functions match the observed light-curves.”
• The delay-time distribution of Type Ia supernovae from Sloan II (2012, methodology): “For the 62 photometrically classified SNe Ia that are from S11, we convert the M15 values, tabulated by S11, to stretch, s, using (Guy et al. 2005, their footnote 7), s = −0.59 M15 + 1.55.”
• TYPE Ia SUPERNOVA LIGHT CURVE INFERENCE: HIERARCHICAL MODELS IN THE OPTICAL AND NEAR-INFRARED (2010, methodology): “Methods include Δm15(B) (Phillips 1993; Hamuy et al. 1996b; Phillips et al. 1999; Prieto et al. 2006), multicolor light curve shapes (MLCS; Riess et al. 1996a, 1998; Jha et al. 2007), “stretch” (Goldhaber et al. 2001), CMAGIC (Wang et al. 2003), SALT (Guy et al. 2005, 2007), and SiFTO (Conley et al.”
• Improved Distances to Type Ia Supernovae with Multicolor Light-Curve Shapes: MLCS2k2 (2006, methodology): “Guy et al. (2005) use an innovative approach to constrain the spectral energy distribution (SED) of SNe Ia, parameterized continuously as a function of color and stretch, and allow for the generation of light-curve templates in arbitrary passbands.”
• Berkeley Supernova Ia Program – I. Observations, data reduction and spectroscopic sample of 582 low-redshift Type Ia supernovae (2012, background): “…Section 5 for more information about SNID and its parameters. bSee Jha et al. (2007) for more information about MLCS2k2 and its parameters. cSee Guy et al. (2005) and Guy et al. (2007) for more information about SALT and SALT2 and their parameters. dSee Section 3.3 for more…”
• A 3% SOLUTION: DETERMINATION OF THE HUBBLE CONSTANT WITH THE HUBBLE SPACE TELESCOPE AND WIDE FIELD CAMERA 3 (2011, methodology): “This quantity is determined for each SN Ia from its multi-band light curves and a light curve fitting algorithm, either from the MLCS2k2 (Jha et al. 2007) or from the SALT-II (Guy et al. 2005) prescription (see Section 4.2 for further discussion).”
• The Supernova Legacy Survey: Measurement of Omega_M, Omega_Lambda,and w from the First Year Data Set (2005, methodology): “This rest-frame-Bmagnitude refers tobservedbrightness, and therefore does not account for brighter-slower and brighterbluer correlations (see Guy et al. 2005 and references therein).”
• Improved Cosmological Constraints from New, Old, and Combined Supernova Data Sets (2008, methodology): “The spectral template based fit method of Guy et al. (2005) fits for the time of maximum, the flux normalization as well as restframe color at maximum defined as c ¼ B V j t¼Bmax þ 0:057 and timescale stretch s.”
• 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.”
• Type Ia Supernovae Are Good Standard Candles in the Near Infrared: Evidence from PAIRITEL (2007, methodology): “While quantitatively uncertain, this RH 0:2 corresponds to an equivalent RV ¼ 1:2, which is in qualitative agreement with previous work on observed supernova color-luminosity behavior (see Perlmutter et al. 1999; Knop et al. 2003; Guy et al. 2005, 2007; Conley et al. 2007).”
• SiFTO: An Empirical Method for Fitting SN Ia Light Curves (2008, methodology): “The details of the complementary lightcurve fitting method (SALT/SALT2) are described in Guy et al. (2005) and G07.”
• Observational probes of cosmic acceleration (2012, methodology): “Many of the algorithms in current use are descendants of the Multicolor Light Curve Shape (MLCS; Riess et al. 1996) or Spectral Adaptive Light Curve Template (SALT; Guy et al. 2005) methods.”
• FIVE-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE OBSERVATIONS: COSMOLOGICAL INTERPRETATION (2008, unknown): “Kowalski et al. (2008) have processed all of these samples using the same light curve fitter called SALT (Guy et al. 2005), which allowed them to combine all the data in a self-consistent fashion.”
• CfA3: 185 TYPE Ia SUPERNOVA LIGHT CURVES FROM THE CfA (2009, methodology): “The impact of adding additional nearby SNe Ia can be seen in Kowalski et al. (2008), who take 49 nearby and 250 faraway SNe Ia from the literature and add eight of their own, using the light-curve fitter SALT (Guy et al. 2005).”
• Cosmological parameter constraints from SDSS luminous red galaxies: a new treatment of large-scale clustering (2009, methodology): “This compilation is drawn from 13 independent data sets processed using the SALT light-curve fitter (Guy et al. 2005) and analysed in a uniform way.”