Uncorrelated measurements of the cosmic expansion history and dark energy from supernovae

By Yun Wang, Max Tegmark. 2005

152 citations recorded by the source corpus.

We present a method for measuring the cosmic expansion history $H(z)$ in uncorrelated redshift bins, and apply it to current and simulated type Ia supernova data assuming spatial flatness. If the matter density parameter ${\ensuremath{\Omega}}_{m}$ can be accurately measured from other data, then the dark-energy density history $X(z)={\ensuremath{\rho}}_{X}(z)/{\ensuremath{\rho}}_{X}(0)$ can trivially be derived from this expansion history $H(z)$. In contrast to customary ``black box'' parameter fitting, our method is transparent and easy to interpret: the measurement of $H(z{)}^{\ensuremath{-}1}$ in a redshift bin is simply a linear combination of the measured comoving distances for supernovae in that bin, making it obvious how systematic errors propagate from input to output. We find the Riess et al. (2004) gold sample to be consistent with the vanilla concordance model where the dark energy is a cosmological constant. We compare two mission concepts for the NASA/DOE Joint Dark-Energy Mission (JDEM), the Joint Efficient Dark-energy Investigation (JEDI), and the Supernova Accelaration Probe (SNAP), using simulated data including the effect of weak lensing (based on numerical simulations) and a systematic bias from K corrections. Estimating $H(z)$ in seven uncorrelated redshift bins, we find that both provide dramatic improvements over current data: JEDI can measure $H(z)$ to about 10% accuracy and SNAP to 30%--40% accuracy.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/58c6a23c1970e0b26321c0878063a3ada2e4d73e

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Citations in the corpus

Smoothing supernova data to reconstruct the expansion history of the universe (2005, background): “…ρDE and H(z) have been suggested in the literature (Daly & Djorgovsky 2003, 2004; Alam et al. 2004; Alam, Sahni & Starobinsky 2004 a; Wang & Mukherjee 2004; Wang & Tegmark 2005), and any c© 0000 RAS, MNRAS 000, 000–000 of these could be used to great advantage in determining the w-probe.”
Observational probes of cosmic acceleration (2012, background): “…evolution are best constrained by a given combination of experiments (Huterer and Starkman, 2003; Hu, 2002a; Huterer and Cooray, 2005; Wang and Tegmark, 2005; Dick et al., 2006; Simpson and Bridle, 2006; de Putter and Linder, 2008; Tang et al., 2011; Crittenden et al., 2009; Mortonson et al.,…”
FIRST-YEAR SLOAN DIGITAL SKY SURVEY-II (SDSS-II) SUPERNOVA RESULTS: CONSTRAINTS ON NONSTANDARD COSMOLOGICAL MODELS (2009, methodology): “Ideally, this constant should be equal to one, corresponding to σH = dH dz ∆z , (11) where σH is the uncertainty in the Hubble parameter and ∆z is the redshift range that each measurement probes, as calculated by Wang & Tegmark (2005).”
Robust Dark Energy Constraints from Supernovae, Galaxy Clustering, and 3 yr Wilkinson Microwave Anisotropy Probe Observations (2006, methodology): “Figure 4 shows the uncorrelated H(z) estimated using only SN Ia data (Wang & Tegmark 2005), and the H(z) corresponding to the X (zi) shown in Figure 3.”
Cosmic dynamics in the era of Extremely Large Telescopes (2008, background): “…Steinhardt 2001; Bassett, Corasaniti & Kunz 2004), these are conceptually undesirable features and several authors have pointed out the importance of taking a cosmographic, model-independent approach to determining the expansion history (e.g. John 2005; Wang & Tegmark 2005; Shapiro & Turner 2006).”
New Hubble Space Telescope Discoveries of Type Ia Supernovae at z ≥ 1: Narrowing Constraints on the Early Behavior of Dark Energy (2006, methodology): “As in Wang & Tegmark (2005), we flux average the data first (n z 1) to remove possible lensing bias.”
Type Ia Supernova Distances at Redshift >1.5 from the Hubble Space Telescope Multi-cycle Treasury Programs: The Early Expansion Rate (2017, methodology): “One proposed method (Wang & Tegmark 2005), which has been employed in some subsequent analyses (Riess et al. 2007; Mortsell & Clarkson 2009; Avgoustidis et al. 2009), seeks direct, independent estimates of E(z) in redshift bins by first converting SN distance moduli into their corresponding…”
Improved Constraints on the Acceleration History of the Universe and the Properties of the Dark Energy (2007, unknown): “This includes the work of Huterer & Starkman (2003), Wang & Tegmark (2004, 2005), Shafieloo et al. (2006), Alam et al. (2004), Nesseris & Perivolaropoulos (2004), Huterer & Cooray (2005), Shapiro&Turner (2006), Turner&Huterer (2007), andAlam et al. (2007), for example.”