The clustering of the SDSS DR7 main Galaxy sample – I. A 4 per cent distance measure at z = 0.15

Ross, Ashley J.; Samushia, Lado; Howlett, Cullan; Percival, Will J.; Burden, A.; Manera, Marc

doi:10.1093/mnras/stv154

Cited by 1,727 publications

(1,564 citation statements)

References 74 publications

(119 reference statements)

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“…We also compare our results to the current precise measurements, such as the results from Planck+WMAP (Planck Collaboration XVI 2013), BAO (Beutler et al 2011;Anderson et al 2014;Kazin et al 2014;Ross et al 2015), and SNe Ia (Conley et al 2011;Suzuki et al 2012). We show them in Table 3.…”

Section: Simultaneous Fittingmentioning

confidence: 80%

Measuring dark energy with theE_iso–E_pcorrelation of gamma-ray bursts using model-independent methods

Wang

Cheng

et al. 2015

A&A

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We use two model-independent methods to standardize long gamma-ray bursts (GRBs) using the E iso − E p correlation (log E iso = a + b log E p ), where E iso is the isotropic-equivalent gamma-ray energy and E p is the spectral peak energy. We update 42 long GRBs and attempt to constrain the cosmological parameters. The full sample contains 151 long GRBs with redshifts from 0.0331 to 8.2. The first method is the simultaneous fitting method. We take the extrinsic scatter σ ext into account and assign it to the parameter E iso . The best-fitting values are a = 49.15 ± 0.26, b = 1.42 ± 0.11, σ ext = 0.34 ± 0.03 and Ω m = 0.79 in the flat ΛCDM model. The constraint on Ω m is 0.55 < Ω m < 1 at the 1σ confidence level. If reduced χ 2 method is used, the best-fit results are a = 48.96 ± 0.18, b = 1.52 ± 0.08, and Ω m = 0.50 ± 0.12. The second method uses type Ia supernovae (SNe Ia) to calibrate the E iso − E p correlation. We calibrate 90 high-redshift GRBs in the redshift range from 1.44 to 8.1. The cosmological constraints from these 90 GRBs are Ω m = 0.23 +0.06 −0.04 for flat ΛCDM and Ω m = 0.18 ± 0.11 and Ω Λ = 0.46 ± 0.51 for non-flat ΛCDM. For the combination of GRB and SNe Ia sample, we obtain Ω m = 0.271 ± 0.019 and h = 0.701 ± 0.002 for the flat ΛCDM and the non-flat ΛCDM, and the results are Ω m = 0.225 ± 0.044, Ω Λ = 0.640 ± 0.082, and h = 0.698 ± 0.004. These results from calibrated GRBs are consistent with that of SNe Ia. Meanwhile, the combined data can improve cosmological constraints significantly, compared to SNe Ia alone. Our results show that the E iso − E p correlation is promising to probe the high-redshift Universe.

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Section: Simultaneous Fittingmentioning

confidence: 80%

Measuring dark energy with theE_iso–E_pcorrelation of gamma-ray bursts using model-independent methods

Wang

Cheng

et al. 2015

A&A

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“…(13). Solid coloured contours show 68% and 95% constraints when additional information is included: BAO data from SDSS and 6DF (Anderson et al 2014;Ross et al 2015;Beutler et al 2011;blue), and the same but fixing the CMB acoustic-scale parameter θ MC to a CMB power spectrum fit (red; θ MC = 1.0408). Solid black contours show the constraint from the Planck CMB power spectra (Planck temperature+low-polarization).…”

Section: Constraints From Cmb Lensing Alonementioning

confidence: 99%

Planck2015 results

Ade

Aghanim

Arnaud

et al. 2016

A&A

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257

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We present the most significant measurement of the cosmic microwave background (CMB) lensing potential to date (at a level of 40σ), using temperature and polarization data from the Planck 2015 full-mission release. Using a polarization-only estimator, we detect lensing at a significance of 5σ. We cross-check the accuracy of our measurement using the wide frequency coverage and complementarity of the temperature and polarization measurements. Public products based on this measurement include an estimate of the lensing potential over approximately 70% of the sky, an estimate of the lensing potential power spectrum in bandpowers for the multipole range 40 ≤ L ≤ 400, and an associated likelihood for cosmological parameter constraints. We find good agreement between our measurement of the lensing potential power spectrum and that found in the ΛCDM model that best fits the Planck temperature and polarization power spectra. Using the lensing likelihood alone we obtain a percent-level measurement of the parameter combination σ 8 Ω 0.25 m = 0.591 ± 0.021. We combine our determination of the lensing potential with the E-mode polarization, also measured by Planck, to generate an estimate of the lensing B-mode. We show that this lensing B-mode estimate is correlated with the B-modes observed directly by Planck at the expected level and with a statistical significance of 10σ, confirming Planck's sensitivity to this known sky signal. We also correlate our lensing potential estimate with the large-scale temperature anisotropies, detecting a cross-correlation at the 3σ level, as expected because of dark energy in the concordance ΛCDM model.

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“…• BAO: the baryon acoustic oscillations measurements from SDSS at z = 0.15 [94], BOSS at z = 0.32 and z = 0.57 [95], and 6dFGS at z = 0.106 [96].…”

mentioning

confidence: 99%

Testing models of vacuum energy interacting with cold dark matter

Zhang

2016

Phys. Rev. D

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We test the models of vacuum energy interacting with cold dark matter and try to probe the possible deviation from the ΛCDM model using current observations. We focus on two specific models, Q = 3βHρΛ and Q = 3βHρc. The data combinations come from the Planck 2013 data, the baryon acoustic oscillations measurements, the type-Ia supernovae data, the Hubble constant measurement, the redshift space distortions data and the galaxy weak lensing data. For the Q = 3βHρc model, we find that it can be tightly constrained by all the data combinations, while for the Q = 3βHρΛ model, there still exist significant degeneracies between parameters. The tightest constraints for the coupling constant are β = −0.026 +0.036 −0.053 (for Q = 3βHρΛ) and β = −0.00045 ± 0.00069 (for Q = 3βHρc) at the 1σ level. For all the fit results, we find that the null interaction β = 0 is always consistent with data. Our work completes the discussion on the interacting dark energy model in the recent Planck 2015 papers. Considering this work together with the Planck 2015 results, it is believed that there is no evidence for the models beyond the standard ΛCDM model from the point of view of possible interaction.Modern cosmology encounters a great puzzle in explaining the late-time cosmic acceleration, as a universe with barotropic or pressureless fluids, evolving according to the laws of general relativity, cannot fit the observational data [1, 2]. This puzzle is phenomenologically solved by introducing a new component with negative pressure, generally called dark energy. However, the fundamental nature of dark energy is still unknown. At present, a cosmological constant Λ with equation of state w = −1 is the simplest candidate of dark energy, which, however, is plagued with the so-called fine-tuning problem and coincidence problem [3,4]. These theoretical problems provide cosmologists with the motivation to consider some complex theories for explaining the cosmic acceleration, such as the dynamical dark energy models or the modified gravity (MG) theories. In particular, in order to solve the coincidence problem, cosmologists have widely investigated the interacting dark energy (IDE) scenario , where dark energy directly interacts with dark matter by exchanging energy and momentum.Regardless of the theoretical problems of Λ, the Λ cold dark matter (ΛCDM) model is still the most competitive cosmological model and is now even taken as a prototype of the standard model in cosmology, as it can excellently fit most of the current data with the least free parameters [63]. Nevertheless, other complex models mentioned above are also not excluded by the observations. Given this fact, we still need to continuously test the validity of the ΛCDM model. Undoubtedly, any deviation from it, if confirmed by observations, would be a major breakthrough in cosmology. In fact, some degree of tension between different observations has been reported for the ΛCDM model since the Planck 2013 results were published [64]. This tension has attracted much interest * Correspon...

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The clustering of the SDSS DR7 main Galaxy sample – I. A 4 per cent distance measure at z = 0.15

Cited by 1,727 publications

References 74 publications

Measuring dark energy with theE_iso–E_pcorrelation of gamma-ray bursts using model-independent methods

Measuring dark energy with theE_iso–E_pcorrelation of gamma-ray bursts using model-independent methods

Planck2015 results

Testing models of vacuum energy interacting with cold dark matter

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The clustering of the SDSS DR7 main Galaxy sample – I. A 4 per cent distance measure at z = 0.15

Cited by 1,727 publications

References 74 publications

Measuring dark energy with theEiso–Epcorrelation of gamma-ray bursts using model-independent methods

Measuring dark energy with theEiso–Epcorrelation of gamma-ray bursts using model-independent methods

Planck2015 results

Testing models of vacuum energy interacting with cold dark matter

Contact Info

Product

Resources

About

Measuring dark energy with theE_iso–E_pcorrelation of gamma-ray bursts using model-independent methods

Measuring dark energy with theE_iso–E_pcorrelation of gamma-ray bursts using model-independent methods