Observational Constraints on the Nature of Dark Energy: First Cosmological Results from the ESSENCE Supernova Survey

Wood‐Vasey, W. M.; Miknaitis, G.; Stubbs, C. W.; Jha, Saurabh W.; Riess, Adam G.; Garnavich, P.; Kirshner, R.; Aguilera, C.; Becker, A.; Blackman, Joshua W.; Blondin, S.; Challis, Peter; Clocchiatti, A.; Conley, A.; Covarrubias, R.; Davis, Tamara M.; Filippenko, A. V.; Foley, R. J.; Garg, Arti; Hicken, M.; Krisciunas, K.; Leibundgut, B.; Li, W.; Matheson, T.; Miceli, Antonino; Narayan, Gautham; Pignata, G.; Prieto, J. L.; Rest, A.; Salvo, M.; Schmidt, B. P.; Smith, R. C.; Sollerman, J.; Spyromilio, J.; Tonry, J.; Suntzeff, Nicholas B.; Zenteno, A.

doi:10.1086/518642

Cited by 803 publications

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“…In any cosmological analysis, one uses the color of a supernova relative to a template expectation (derived from a training set) to infer, and correct for, a correlation between color and apparent magnitude arising from dust and/or intrinsic color variations. In the analysis of Wood-Vasey et al (2007), different priors about host galaxy extinction change the inferred value of w by amounts comparable to the statistical error. When the ratio of extinction to reddening is treated as a free parameter in the cosmological fits, the derived values are typically quite far from those measured for Galactic interstellar dust, e.g., R V ≡ A V /E(B − V ) = 1.5 − 2.5 (Hicken et al 2009b;Kessler et al 2009;Sullivan et al 2011) instead of the mean R V = 3.1 found in the diffuse interstellar medium of the Milky Way (Cardelli et al, 1989).…”

Section: The Current State Of Playmentioning

confidence: 98%

“…Prominent examples include the supernova and weak lensing programs of the CFHT Legacy Survey (CFHTLS; Conley et al 2011;Semboloni et al 2006a;Heymans et al 2012b), the ESSENCE supernova survey (Wood-Vasey et al, 2007), BAO measurements from the Sloan Digital Sky Survey (SDSS; Eisenstein et al 2005;Percival et al 2010;Padmanabhan et al 2012), and the SDSS-II supernova survey . These have been complemented by extensive multi-wavelength studies of local and high-redshift supernovae such as the Carnegie Supernova Project (Hamuy et al, 2006;Freedman et al, 2009), by systematic searches for z > 1 supernovae with Hubble Space Telescope Suzuki et al, 2012), by dark energy constraints from the evolution of X-ray or optically selected clusters (Henry et al, 2009;Vikhlinin et al, 2009;Rozo et al, 2010), by improved measurements of the Hubble constant (Riess et al, , 2011Freedman et al, 2012), and by CMB data from the WMAP satellite (Bennett et al, 2003;Larson et al, 2011) and from ground-based experiments that probe smaller angular scales.…”

Section: Looking Forwardmentioning

confidence: 99%

“…The largest high-redshift (z ≈ 0.4 − 1.0) data sets are those from the ESSENCE survey (Wood-Vasey et al 2007; Narayan et al, in prep. ; ∼200 spectroscopically confirmed Type Ia SNe) and the CFHT Supernova Legacy Survey (SNLS; Astier et al 2006;Conley et al 2011;Sullivan et al 2011; ∼500 spectroscopically confirmed Type Ia SNe in the three-year data set SNLS3).…”

Section: The Current State Of Playmentioning

confidence: 99%

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Observational probes of cosmic acceleration

et al. 2013

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The accelerating expansion of the universe is the most surprising cosmological discovery in many decades, implying that the universe is dominated by some form of "dark energy" with exotic physical properties, or that Einstein's theory of gravity breaks down on cosmological scales. The profound implications of cosmic acceleration have inspired ambitious efforts to understand its origin, with experiments that aim to measure the history of expansion and growth of structure with percent-level precision or higher. We review in detail the four most well established methods for making such measurements: Type Ia supernovae, baryon acoustic oscillations (BAO), weak gravitational lensing, and the abundance of galaxy clusters. We pay particular attention to the systematic uncertainties in these techniques and to strategies for controlling them at the level needed to exploit "Stage IV" dark energy facilities such as BigBOSS, LSST, Euclid, and WFIRST. We briefly review a number of other approaches including redshift-space distortions, the Alcock-Paczynski effect, and direct measurements of the Hubble constant H 0 . We present extensive forecasts for constraints on the dark energy equation of state and parameterized deviations from General Relativity, achievable with Stage III and Stage IV experimental programs that incorporate supernovae, BAO, weak lensing, and cosmic microwave background data. We also show the level of precision required for clusters or other methods to provide constraints competitive with those of these fiducial programs. We emphasize the value of a balanced program that employs several of the most powerful methods in combination, both to cross-check systematic uncertainties and to take advantage of complementary information. Surveys to probe cosmic acceleration produce data sets that support a wide range of scientific investigations, and they continue the longstanding astronomical tradition of mapping the universe in ever greater detail over ever larger scales.

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Section: The Current State Of Playmentioning

confidence: 98%

Section: Looking Forwardmentioning

confidence: 99%

Section: The Current State Of Playmentioning

confidence: 99%

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Observational probes of cosmic acceleration

et al. 2013

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“…The accelerated expansion is currently widely attributed to the existence of a "dark energy" component, which is compatible with Einsteinʼs cosmological constant. Over the last decade, the sample of SNe Ia has increased dramatically (e.g., Astier et al 2006;Wood-Vasey et al 2007;Bailey et al 2008;Kowalski et al 2008;Balland et al 2009;Freedman et al 2009;Hicken et al 2009;Kessler et al 2009;Amanullah et al 2010;Contreras et al 2010;Suzuki et al 2012;Betoule et al 2014;Rest et al 2014), and it now comprises several hundred spectroscopically confirmed SNe Ia. Since SNe Ia probe the low-redshift universe, they are ideal tools to measure the properties of dark energy.…”

Section: Introductionmentioning

confidence: 99%

BAHAMAS: NEW ANALYSIS OF TYPE Ia SUPERNOVAE REVEALS INCONSISTENCIES WITH STANDARD COSMOLOGY

Shariff

Jiao

Trotta

et al. 2016

ApJ

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We present results obtained by applying our BAyesian HierArchical Modeling for the Analysis of Supernova cosmology (BAHAMAS) software package to the 740 spectroscopically confirmed supernovae of type Ia (SNe Ia) from the "Joint Light-curve Analysis" (JLA) data set. We simultaneously determine cosmological parameters and standardization parameters, including corrections for host galaxy mass, residual scatter, and object-by-object intrinsic magnitudes. Combining JLA and Planck data on the cosmic microwave background, we find significant discrepancies in cosmological parameter constraints with respect to the standard analysis: we find W =  0.399 0.027 m , s 2.8 higher than previously reported, and = - w 0.910 0.045, s 1.6 higher than the standard analysis. We determine the residual scatter to be s =  0.104 0.005 res . We confirm (at the 95% probability level) the existence of two subpopulations segregated by host galaxy mass, separated at, differing in mean intrinsic magnitude by 0.055 ± 0.022 mag, lower than previously reported. Cosmological parameter constraints, however, are unaffected by the inclusion of corrections for host galaxy mass. We find s4 evidence for a sharp drop in the value of the color correction parameter, ( ) b z , at a redshift =  z 0.662 0.055 t . We rule out some possible explanations for this behavior, which remains unexplained.

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“…Recently direct SN searches, for example with the Hubble space telescope (HST) (Knop et al, 2003), have obtained high quality light curves and are able to constrain the cosmological parameters independently of other datasets. Recent supernovae observations of the distance modulus versus redshift (see Appendix A.1) from the Supernova Legacy Survey (SNLS) and the ESSENCE survey (Miknaitis et al, 2007;Wood-Vasey et al, 2007) are shown in Fig. 1.1.…”

Section: The Accelerating Expansion Of the Universementioning

confidence: 99%

Simulations of Dark Energy Cosmologies

Jennings

2012

Springer Theses

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The full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-pro t purposes provided that:• a full bibliographic reference is made to the original source• a link is made to the metadata record in Durham E-Theses• the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders. No part of this thesis has been submitted elsewhere for any other degree or qualification.The work of others has been duly acknowledged.The copyright of this thesis rests with the author. No quotations from it should be published without the author's prior written consent and information derived from it should be acknowledged. AbstractFuture galaxy redshift surveys will make high precision measurements of the cosmic expansion history and the growth of structure which will potentially allow us to distinguish between different scenarios for the accelerating expansion of the Universe. In this thesis we study the nonlinear growth of cosmic structure in different dark energy models, using ultra-large volume N-body simulations. We measure key observables such as the growth of large scale structure, the halo mass function and baryonic acoustic oscillations.We study the power spectrum in redshift space in ΛCDM and quintessence dark energy models and test predictions for the form of the redshift space distortions. An improved model for the redshift space power spectrum, including the non-linear velocity divergence power spectrum, is presented. We have found a density-velocity relation which is cosmology independent and which relates the non-linear velocity divergence spectrum to the non-linear matter power spectrum. We provide a formula which generates the non-linear velocity divergence P(k) at any redshift, using only the non-linear matter power spectrum and the linear growth factor at the desired redshift. We also demonstrate for the first time that competing cosmological models with identical expansion histories -one with a scalar field and the other with a time-dependent change to Newton's gravitational constant -can indeed be distinguished by a measurement of the rate at which structures grow.Our calculations show that linear theory models for the power spectrum in redshift space fail to recover the correct growth rate on surprisingly large scales, leading to catastrophic systematic errors. Improved theoretical models, which have been calibrated against simulations, are needed to exploit the exquisitely accurate clustering measurements expected from future surveys.

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Observational Constraints on the Nature of Dark Energy: First Cosmological Results from the ESSENCE Supernova Survey

Cited by 803 publications

References 133 publications

Observational probes of cosmic acceleration

Observational probes of cosmic acceleration

BAHAMAS: NEW ANALYSIS OF TYPE Ia SUPERNOVAE REVEALS INCONSISTENCIES WITH STANDARD COSMOLOGY

Simulations of Dark Energy Cosmologies

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