Timescale Stretch Parameterization of Type Ia Supernova B-Band Light Curves

By G. Goldhaber, D. Groom, A. Kim, G. Aldering, P. Astier, A. Conley, S. Deustua, R. Ellis, S. Fabbro, A. Fruchter and 16 more. 2001

317 citations recorded by the source corpus.

R-band intensity measurements along the light curve of Type Ia supernovae (SNe Ia) discovered by the Supernova Cosmology Project (SCP) are fitted in brightness to templates allowing a free parameter the time-axis width factor w ≡ s(1 + z). The data points are then individually aligned in the time axis, normalized, and K-corrected back to the rest frame, after which the nearly 1300 normalized intensity measurements are found to lie on a well-determined common rest-frame B-band curve, which we call the "composite curve." The same procedure is applied to 18 low-redshift Calán/Tololo SNe with z < 0.11; these nearly 300 B-band photometry points are found to lie on the composite curve equally well. The SCP search technique produces several measurements before maximum light for each supernova. We demonstrate that the linear stretch factor, s, which parameterizes the light-curve timescale, appears independent of z, and applies equally well to the declining and rising parts of the light curve. In fact, the B-band template that best fits this composite curve fits the individual supernova photometry data when stretched by a factor s with χ2/dof ≈ 1—thus, as well as any parameterization can, given the current data sets. The measurement of the date of explosion, however, is model dependent and not tightly constrained by the current data. We also demonstrate the 1 + z light-curve time-axis broadening expected from cosmological expansion. This argues strongly against alternative explanations, such as tired light, for the redshift of distant objects.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/c6e258f8ee3f15e13bce59809e1d6016550a71f7

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. A. Filippenko
2. A. Riess
3. R. Kirshner
4. K. Luhman
5. S. Jha
6. S. Smartt
7. N. Smith
8. Weidong Li

In Nuclear and High Energy Physics

1. S. Smartt
2. R. Kirshner
3. A. Filippenko
4. A. Riess
5. S. Jha
6. E. Berger
7. Weidong Li
8. B. Leibundgut

Citations in the corpus

• The Luminosity of SN 1999by in NGC 2841 and the Nature of “Peculiar” Type Ia Supernovae (2001, methodology): “Riess et al. (1999b) find that for a nominal SN Ia [ m15(B) ¼ 1:1] the interval from explosion to T(Bmax) is 19:5 0:2 days, and this is consistent with SNe Ia observed at high redshift when a stretch correction is applied on the basis of the lightcurve shape (Goldhaber et al. 2001).”
• Improved Cosmological Constraints from New, Old, and Combined Supernova Data Sets (2008, background): “It is worth noting that by construction, the stretch in SALT has a related meaning to the conventional time-axis stretch (Perlmutter et al. 1997; Goldhaber et al. 2001).”
• The Supernova Legacy Survey: Measurement of Omega_M, Omega_Lambda,and w from the First Year Data Set (2005, methodology): “…in Perlmutter et al. (1997): it parameterizes the brighter-slower relation, originally described in Phillips (1993), by stretching the time axis ofa unique light-curve template;s = 1 is defined in rest-frameB for the time interval−15 to+35 days using the Goldhaber et al. (2001) B-band template.”
• The ESSENCE Supernova Survey: Survey Optimization, Observations, and Supernova Photometry (2007, methodology): “The template light curve is representative of a normal SN Iawith m15 ¼ 1:1mag (Phillips 1993), or stretch ¼ 1 (Goldhaber et al. 2001), and was constructed fromwell-sampled light curves of low-redshift SNe Ia (Prieto et al. 2006).”
• UBVRI Light Curves of 44 Type Ia Supernovae (2005, methodology): “In fitting our stretch templates to the data, we generally follow the methodology of Goldhaber et al. (2001) as applied in their analysis of the Calán/Tololo sample (Hamuy et al. 1996a).”
• 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).”
• Type Ia Supernovae Are Good Standard Candles in the Near Infrared: Evidence from PAIRITEL (2007, methodology): “…rest on a foundation of photometric and spectroscopic similarities between high- and low-redshift SNe Ia (Hamuy et al. 1996; Riess et al. 1999; Goldhaber et al. 2001; Hook et al. 2005; Blondin et al. 2006; Jha et al. 2006; Conley et al. 2006; Garavini et al. 2007; Garg et al. 2007; Bronder et…”
• The Supernova Legacy Survey 3-year sample: Type Ia supernovae photometric distances and cosmological constraints , (2010, background): “Historically, light curve templates were built in a limited set of filters from a sample of nearby SNe (see for instance Goldhaber et al. 2001).”
• SALT2: using distant supernovae to improve the use of type Ia supernovae as distance indicators (2007, methodology): “…can be converted into a stretch factor3, whose actual value depends on the reference light-curve template used, here the one of SALT and of Goldhaber et al. (2001) (B-band light curve template “Parab -18”, G01); or into ∆m15 (Phillips 1993) using the following transformations: s (S ALT )…”
• SPECTRA AND HUBBLE SPACE TELESCOPE LIGHT CURVES OF SIX TYPE Ia SUPERNOVAE AT 0.511 < z < 1.12 AND THE UNION2 COMPILATION (2010, methodology): “Several methods of combining this information into an accurate measure of the relative distance have been used (Riess et al. 1996; Goldhaber et al. 2001; Wang et al. 2003; Guy et al. 2005, 2007; Jha et al. 2007; Conley et al. 2008).”
• Expanding Confusion: Common Misconceptions of Cosmological Horizons and the Superluminal Expansion of the Universe (2003, background): “Leibundgut et al. (1996), Riess et al. (1997) and Goldhaber et al. (1997, 2001) do provide excellent evidence that expansion is a good explanation for cosmological redshifts.”
• SiFTO: An Empirical Method for Fitting SN Ia Light Curves (2008, methodology): “Light-curve shape The SiFTO model for light-curve shape is based on the stretch parameterization (Perlmutter et al. 1997; Goldhaber et al. 2001).”
• CfA3: 185 TYPE Ia SUPERNOVA LIGHT CURVES FROM THE CfA (2009, methodology): “…light-curve shape) and have been used to measure the expansion history of the universe (e.g., Phillips 1993; Riess et al. 1996; Hamuy et al. 1996a; Goldhaber et al. 2001; Jha et al. 2007), giving rise to the startling conclusion that the universe is accelerating (e.g., Riess et al. 1998;…”
• TYPE Ia SUPERNOVA LIGHT CURVE INFERENCE: HIERARCHICAL MODELS IN THE OPTICAL AND NEAR-INFRARED (2010, methodology): “…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. 2008).”
• Determining the Type, Redshift, and Age of a Supernova Spectrum (2006, unknown): “For this comparison to make sense we must correct the light-curve age for the (1 + z) time-dilation factor expected in an expanding universe (Wilson 1939; Rust 1974; Leibundgut et al. 1996; Goldhaber et al. 2001).”
• K‐Corrections and Extinction Corrections for Type Ia Supernovae (2002, unknown): “The B- and V -band light curves come from the data of Riess et al. (1999a) and the R, I light curves from Knop (2002) (see also Goldhaber et al. (2001) for comparable B-band templates).”
• IMPROVED DARK ENERGY CONSTRAINTS FROM ∼100 NEW CfA SUPERNOVA TYPE Ia LIGHT CURVES (2009, background): “…candles and the most useful distance indicators at cosmological scales (e.g., Phillips 1993; Hamuy et al. 1996a; Riess, Press, & Kirshner 1996; Perlmutter et al. 1997; Jha et al. 1999; Goldhaber et al. 2001; Guy et al. 2005; Jha, Riess, & Kirshner 2007; Guy et al. 2007; Conley et al. 2008).”
• COSMOLOGICAL CONSTRAINTS FROM MEASUREMENTS OF TYPE Ia SUPERNOVAE DISCOVERED DURING THE FIRST 1.5 yr OF THE Pan-STARRS1 SURVEY (2013, background): “Since then, new approaches and new algorithms have improved lightcurve fitting so that well-observed SN Ia have individual luminosity distances good to 5% (e.g., MLCS2K2, Jha et al. 2007; Stretch, Goldhaber et al. 2001; SALT, Guy et al. 2007; SiFTO, Conley et al. (2008); and BayeSN, Mandel et al. 20”