Interferometric Measurement of Resonance Transition Wavelengths in C [CSC]iv[/CSC], S[CLC]i[/CLC] [CSC]iv[/CSC], A[CLC]l[/CLC] [CSC]iii[/CSC], A[CLC]l[/CLC] [CSC]ii[/CSC], and S[CLC]i[/CLC] [CSC]ii[/CSC]

Griesmann, Ulf; Kling, Rainer

doi:10.1086/312741

Cited by 53 publications

(67 citation statements)

References 18 publications

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“…This gives us the required number of components to be used in the fit and an initial guess of N, b and z for each component. Griesmann & Kling (2000). b Dzuba et al (1999a).…”

Section: Discussionmentioning

confidence: 99%

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Probing the time-variation of the fine-structure constant: Results based on Si IV doublets from a UVES sample

Chand¹,

Petitjean

Srianand³

et al. 2005

A&A

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Abstract. We report a new constraint on the variation of the fine-structure constant based on the analysis of 15 Si  doublets selected from a ESO-UVES sample. We find ∆α/α = (+0.15 ± 0.43) × 10 −5 over a redshift range of 1.59 ≤ z ≤ 2.92 which is consistent with no variation in α. This result represents a factor of three improvement on the constraint on ∆α/α based on Si  doublets compared to the published results in the literature. The alkali doublet method used here avoids the implicit assumptions used in the many-multiplet method that chemical and ionization inhomogeneities are negligible and isotopic abundances are close to the terrestrial value.

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“…This gives us the required number of components to be used in the fit and an initial guess of N, b and z for each component. Griesmann & Kling (2000). b Dzuba et al (1999a).…”

Section: Discussionmentioning

confidence: 99%

“…In this paper our motivation is to improve the ∆α/α measurements by using the alkali doublets detected in our UVES data of higher S/N and resolution. Si  is used instead of C  because wavelengths are better known for Si  (Griesmann & Kling 2000;Petitjean & Aracil 2004a) and q coefficients are larger (see Table 2). …”

Section: Introductionmentioning

confidence: 99%

Probing the time-variation of the fine-structure constant: Results based on Si IV doublets from a UVES sample

Chand¹,

Petitjean

Srianand³

et al. 2005

A&A

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show abstract

“… a Hannemann et al (2006); b Salumbides et al (2006); c Batteiger et al (2009); d Griesmann & Kling (2000); e Berengut, Dzuba & Flambaum (2003); f 1.4 × (Massshift); g Aldenius, Johansson & Murphy (2006); h Berengut, Flambaum & Kozlov (2008); i Blackwell‐Whitehead et al (2005); j Porsev, Kozlov & Reimers (2009); k S. Johansson (private communication); l Pickering et al (2000); m Matsubara et al (2003b); n Dixit et al (2008); o Matsubara et al (2003a). …”

Section: Quasar Spectra and Laboratory Wavelength Transitionsmentioning

confidence: 99%

Spatial variation in the fine-structure constant - new results from VLT/UVES

King¹,

Webb²,

Murphy³

et al. 2012

Monthly Notices of the Royal Astronomical Society

268

431

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Quasar absorption lines provide a precise test of whether the fine‐structure constant, α, is the same in different places and through cosmological time. We present a new analysis of a large sample of quasar absorption‐line spectra obtained using the Ultraviolet and Visual Echelle Spectrograph (UVES) on the Very Large Telescope (VLT) in Chile. We apply the many‐multiplet method to derive values of Δα/α≡ (αz−α0)/α0 from 154 absorbers, and combine these values with 141 values from previous observations at the Keck Observatory in Hawaii. In the VLT sample, we find evidence that α increases with increasing cosmological distance from Earth. However, as previously shown, the Keck sample provided evidence for a smaller α in the distant absorption clouds. Upon combining the samples, an apparent variation of α across the sky emerges which is well represented by an angular dipole model pointing in the direction RA = 17.3 ± 1.0 h and Dec. =−61°± 10°, with amplitude . The dipole model is required at the 4.1σ statistical significance level over a simple monopole model where α is the same across the sky (but possibly different from the current laboratory value). The data sets reveal remarkable consistencies: (i) the directions of dipoles fitted to the VLT and Keck samples separately agree; (ii) the directions of dipoles fitted to z < 1.6 and z > 1.6 cuts of the combined VLT+Keck samples agree; and (iii) in the equatorial region of the dipole, where both the Keck and VLT samples contribute a significant number of absorbers, there is no evidence for inconsistency between Keck and VLT. The amplitude of the dipole is clearly larger at higher redshift. Assuming a dipole‐only (i.e. no‐monopole) model whose amplitude grows proportionally with ‘lookback‐time distance’ (r=ct, where t is the lookback time), the amplitude is (1.1 ± 0.2) × 10−6 GLyr−1 and the model is significant at the 4.2σ confidence level over the null model (Δα/α≡ 0). We apply robustness checks and demonstrate that the dipole effect does not originate from a small subset of the absorbers or spectra. We present an analysis of systematic effects, and are unable to identify any single systematic effect which can emulate the observed variation in α. To the best of our knowledge, this result is not in conflict with any other observational or experimental result.

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“…However, intra-order distortions of the wavelength scale, such as those discovered by Griest et al [31] for Keck-HIRES, are a source of systematic error (see below). Uncertainty in the line rest wavelengths is an important limitation for this method, and has restricted its recent application to the Siiv 1393/1402 doublet, whose wavelengths have been accurately measured in the laboratory [30]. Improved determinations of the rest wavelengths of other doublets, e.g.…”

Section: The Alkali Doublet Methodsmentioning

confidence: 99%

Probing fundamental constant evolution with redshifted spectral lines

Kanekar¹

2012

Vignettes in Gravitation and Cosmology

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Comparisons between the redshifts of spectral lines from cosmologically-distant galaxies can be used to probe temporal changes in lowenergy fundamental constants like the fine structure constant and the protonelectron mass ratio. In this article, I review the status of this field, including the best current results from techniques using this approach, the advantages and disadvantages of the different methods, and the possibilities for progress with future astronomical studies of fundamental constant evolution. IntroductionAn implicit assumption in the standard model of particle physics is that coupling constants and the ratios of particle masses do not depend on space and time. This assumption typically breaks down in higher-dimensional theories that attempt to unify the standard model with general relativity (e.g. 61, 15). A fairly generic prediction of these models is that fundamental "constants" like the fine structure constant should show space-time variation. This is one of the few low-energy predictions of theoretical extensions of the standard model and general relativity, and has hence attracted much experimental and observational attention [for recent reviews, see, e.g., Uzan [93], García-Berro et al. [28]]. A wide variety of methods have been used to test the possibility of 51 Vignettes in Gravitation and Cosmology Downloaded from www.worldscientific.com by KAINAN UNIVERSITY on 01/09/15. For personal use only.

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Interferometric Measurement of Resonance Transition Wavelengths in C [CSC]iv[/CSC], S[CLC]i[/CLC] [CSC]iv[/CSC], A[CLC]l[/CLC] [CSC]iii[/CSC], A[CLC]l[/CLC] [CSC]ii[/CSC], and S[CLC]i[/CLC] [CSC]ii[/CSC]

Cited by 53 publications

References 18 publications

Probing the time-variation of the fine-structure constant: Results based on Si IV doublets from a UVES sample

Probing the time-variation of the fine-structure constant: Results based on Si IV doublets from a UVES sample

Spatial variation in the fine-structure constant - new results from VLT/UVES

Probing fundamental constant evolution with redshifted spectral lines

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