Is the baryon acoustic oscillation peak a cosmological standard ruler?

Roukema, Boudewijn F.; Buchert, Thomas; Fujii, Hirokazu; Ostrowski, Jan J.

doi:10.1093/mnrasl/slv159

Cited by 23 publications

(22 citation statements)

References 52 publications

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“…The latter type of estimate appears to be convergent with respect to increasing data quality and improved analysis (Blanchard et al 2003;Hunt & Sarkar 2007;Nadathur & Sarkar 2011). As mentioned above, this lower estimate of H bg 0 yields a bg0 = 0.90 ± 0.01, improving the correspondence between the BAO peak shift (shrinkage across superclusters; Roukema et al 2015Roukema et al , 2016) and a bg0 .…”

Section: Astrophysical Age Of Universe Estimates As a Test Of Inhomogsupporting

confidence: 52%

“…pec_expan-bbl which is slightly stronger than the ≈ 10% shrinkage in the BAO peak location detected for Sloan Digital Sky Survey Luminous Red Galaxy pairs whose paths cross superclusters in either the Nadathur & Hotchkiss (2014) or Liivamägi et al (2012) supercluster catalogues (Roukema, Buchert, Ostrowski, & France 2015;Roukema, Buchert, Fujii, & Ostrowski 2016). This suggests that BAO-peak-scale regions crossing superclusters could be considered as a slightly expanded present-day physical realisation of the EdS model extrapolated from early epochs, which we refer to in this paper as our background model.…”

Section: λCdm As An Observational Proxymentioning

confidence: 71%

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The background Friedmannian Hubble constant in relativistic inhomogeneous cosmology and the age of the Universe

Roukema

Mourier

Buchert

et al. 2017

A&A

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Context. In relativistic inhomogeneous cosmology, structure formation couples to average cosmological expansion. A conservative approach to modelling this assumes an Einstein-de Sitter model (EdS) at early times and extrapolates this forward in cosmological time as a "background model" against which average properties of today's Universe can be measured. Aims. This requires adopting an early-epoch-normalised background Hubble constant H bg 1 .Methods. Here, we show that the ΛCDM model can be used as an observational proxy to estimate H bg 1 rather than choose it arbitrarily. We assume (i) an EdS model at early times; (ii) a zero dark energy parameter; (iii) bi-domain scalar averaging-division of the spatial sections into over-and underdense regions; and (iv) virialisation (stable clustering) of collapsed regions. Results. We find H bg 1 = 37.7 ± 0.4 km/s/Mpc (random error only) based on a Planck ΛCDM observational proxy. Conclusions. Moreover, since the scalar-averaged expansion rate is expected to exceed the (extrapolated) background expansion rate, the expected age of the Universe should be much less than 2/(3H bg 1 ) = 17.3 Gyr. The maximum stellar age of Galactic Bulge microlensed low-mass stars (most likely: 14.7 Gyr; 68% confidence: 14.0-15.0 Gyr) suggests an age about a Gyr older than the (no-backreaction) ΛCDM estimate.

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Section: Astrophysical Age Of Universe Estimates As a Test Of Inhomogsupporting

confidence: 52%

Section: λCdm As An Observational Proxymentioning

confidence: 71%

The background Friedmannian Hubble constant in relativistic inhomogeneous cosmology and the age of the Universe

Roukema

Mourier

Buchert

et al. 2017

A&A

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“…If the environment dependence were genuinely an environment-dependent effect, then it should strengthen as the required overlap between galaxy pairs and superclusters increased. This is indeed the case, as was shown in the recent work presented at the meeting, with the shift increasing up to 10% of the peak location [53]. This presently only qualifies as a qualitative inconsistency with ΛCDM.…”

Section: Recent Observational Resultssupporting

confidence: 53%

“…On a scale up to a little less than 1 h −1 Gpc, Roukema presented recent SDSS DR7 work with Buchert, Fujii and Ostrowski [53] extending previous work [52] that showed that the ≈ 105 h −1 Mpc BAO peak location, normally thought of as a comoving standard ruler, is shrunk by a fraction of 6% across SDSS DR7 superclusters. This is expected from scalar averaging, which can be seen as a generalrelativistically more careful generalisation of the FLRW model [88][89][90], but has not been predicted in the ΛCDM model.…”

Section: Recent Observational Resultsmentioning

confidence: 65%

Observational challenges for the standard FLRW model

Buchert

Coley

Kleinert

et al. 2016

Int. J. Mod. Phys. D

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110

109

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We summarise some of the main observational challenges for the standard FriedmannLemaître-Robertson-Walker cosmological model and describe how results recently presented in the parallel session "Large-scale Structure and Statistics" (DE3) at the "Fourteenth Marcel Grossman Meeting on General Relativity" are related to these challenges.Keywords: large-scale structure; cosmic microwave background; statistics; generalrelativistic effects PACS numbers: 98.80.Es, 98.80.Jk, 95.36.+x, Observational Challenges for the ΛCDM ModelDespite the many well-known successes of the FLRW model with its standard parameter values, henceforth denoted the ΛCDM model, there is a wide range of observations with which it significantly disagrees. The statistical significance of these disagreements is very often debated from a Bayesian perspective. If the ΛCDM is accepted as being consistent with general relativity, then one must contend with a posteriori statistics, also called the look elsewhere effect, which globally requires ǎ Sidàk-Bonferonni correction [1] for assessing overall statistical significance. On the other hand, interpretation of structure formation within the ΛCDM model is to a large degree based on Newtonian physics-N -body simulations are widely seen as providing state-of-the-art ways of comparing the FLRW model to observational catalogues-but in comparison to general relativity, the former should be assigned an extremely weak prior.a Although precise tests of general relativity have led to * BFR: During invited lectureship. a For example, Keplerian orbits are disfavoured in relation to general-relativistic orbits at a significance level of more than 100σ [2] based on the periastron decay of the Hulse-Taylor pulsar B1913+16 [3] (See Fig. 2

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“…This is indeed the case, as was shown in the recent work presented at the meeting, with the shift increasing up to 10% of the peak location. 53 This presently only qualifies as a qualitative inconsistency with ΛCDM. Future work should confirm whether or not the environmentdependent BAO peak location shift is quantitatively consistent with ΛCDM.…”

mentioning

confidence: 99%