Issue 
A&A
Volume 526, February 2011



Article Number  A96  
Number of page(s)  9  
Section  Cosmology (including clusters of galaxies)  
DOI  https://doi.org/10.1051/00046361/201014835  
Published online  04 January 2011 
Robust limit on a varying protontoelectron mass ratio from a single H_{2} system
^{1}
Hamburger Sternwarte, Universität Hamburg,
Gojenbergsweg 112,
21029
Hamburg,
Germany
email: mwendt@hs.unihamburg.de
^{2}
Osservatorio Astronomico di Trieste, via G. B. Tiepolo
11, 34131
Trieste,
Italy
Received: 21 April 2010
Accepted: 29 November 2010
Context. The variation of the dimensionless fundamental physical constant μ = m_{p}/m_{e} can be checked through observation of Lyman and Werner lines of molecular hydrogen in the spectra of distant QSOs. Only few, at present four, systems have been used for the purpose providing different results between the different authors.
Aims. Our intention is to asses the accuracy of the investigation concerning a possible variation of the fundamental physical constant μ = m_{p}/m_{e} and to provide more robust results. The goal in mind is to resolve the current controversy on variation of μ and devise explanations for the different findings.
Methods. The demand for precision requires a deep understanding of the errors involved. Selfconsistency in data analysis and effective techniques to handle unknown systematic errors are essential. An analysis based on independent data sets of QSO 0347383 is put forward and new approaches for some of the steps involved in the data analysis are introduced. In this work we analyse two independent sets of observations of the same absorption system and for the first time we apply corrections for the observed offsets between discrete spectra mainly caused by slit illumination effects.
Results. Drawing on two independent observations of a single absorption system in QSO 0347383 our detailed analysis yields Δμ/μ = (15 ± (9_{stat} + 6_{sys})) × 10^{6} at z_{abs} = 3.025. Based on the scatter of the measured redshifts and the corresponding low significance of the redshiftsensitivity correlation we estimate the limit of accuracy of Δμ measurements to ~300 m s^{1}, consisting of roughly 180 m s^{1} due to the uncertainty of the absorption line fit and about 120 m s^{1} allocated to systematics.
Conclusions. Current analyses tend to underestimate the impact of systematic errors. This work presents alternative approaches to handle systematics and introduces methods required for precision analysis of QSO spectra available in the near future.
Key words: cosmology: observations / quasars: absorption lines / quasars: individual: QSO 0347383
© ESO, 2011
1. Introduction
The standard model of particle physics (SMPP) is very successful and its predictions are tested to high precision in laboratories around the world. SMPP needs several dimensionless fundamental constants, such as coupling constants and mass ratios, whose values cannot be predicted and must be established through experiment (Fritzsch 2009). Our confidence in their constancy stems from laboratory experiments over human timescales but variations might have occurred over the 14 billionyear history of the Universe while remaining undetectably small today. Indeed, in theoretical models seeking to unify the four forces of nature, the coupling constants vary naturally on cosmological scales.
The protontoelectron mass ratio, μ = m_{p}/m_{e} has been the subject of numerous studies. The mass ratio is sensitive primarily to the quantum chromodynamic scale. The Λ_{QCD} scale should vary considerably faster than that of quantum electrodynamics Λ_{QED}. As a consequence, the secular change in the protontoelectron mass ratio, if any, should be larger than that of the fine structure constant. Hence, μ is a promising candidate to search for possible cosmological variations of the fundamental constants.
The present value of the protontoelectron mass ratio is μ = 1836.15267261(85) (Mohr & Taylor 2000). Laboratory experiments by comparing the rates between clocks based on hyperfine transitions in atoms with a different dependence on μ restrict the timedependence of μ at the level of yr^{1} (Blatt et al. 2008).
A probe of the variation of μ is obtained by comparing rotational versus vibrational modes of molecules as first suggested by Thompson (1975). The method is based on the fact that the wavelengths of vibrorotational lines of molecules depend on the reduced mass, M, of the molecule. The energy difference between two consecutive levels of the rotational spectrum of a diatomic molecule scales with the reduced mass M, whereas the energy difference between two adjacent levels of the vibrational spectrum is proportional to (M)^{1/2}: (1)with c_{e}, c_{v} and c_{r} as constant factors for the electronic, vibrational and rotational contribution, respectively. Consequently, by studying the Lyman and Werner transitions of molecular hydrogen we may obtain information about a change in μ. The observed wavelength λ_{obs,i} of any given line in an absorption system at the redshift z differs from the local restframe wavelength λ_{0,i} of the same line in the laboratory according to the relation
(2)where K_{i} is the sensitivity coefficient of the ith component computed theoretically for the Lyman and Werner bands of the H_{2} molecule. Using this expression, the cosmological redshift of a line can be distinguished from the shift due to a variation of μ.
This method was used to obtain upper bounds on the secular variation of the electrontoproton mass ratio from observations of distant absorption systems in the spectra of quasars at several redshifts. The quasar absorption system towards QSO 0347383 was first studied by us using highresolution spectra obtained with the very large telescope/ultravioletvisual echelle spectrograph (VLT^{1}/UVES^{2}) commissioning data we derived a first stringent bound at (−1.8 ± 3.8) × 10^{5} (Levshakov et al. 2002a). Subsequent measures of the quasar absorption systems of QSO 0347382 and QSO 1232+082 provided hints for a variation (2.4 ± 0.6) × 10^{5}, i.e. at 3.5σ (Reinhold et al. 2006; Ivanchik et al. 2005; Ubachs et al. 2007). The new analysis used additional highresolution spectra and updated laboratory data of the energy levels and of the rest frame wavelengths of the H_{2}molecule.
However, more recently King et al. (2008), Wendt & Reimers (2008) and Thompson et al. (2009a) reevaluated data of the same system and report a result in agreement with no variation. The more stringent limits on Δμ/μ have been found at Δμ/μ = (2.6 ± 3.0_{stat}) × 10^{6} from the combination of three H_{2} systems (King et al. 2008) and a fourth one have provided Δμ/μ = (+5.6 ± 5.5_{stat} ± 2.9_{sys}) × 10^{6} (Malec et al. 2010).
This work is motivated on one side by the use of a new data set available in the ESO data archive and previously overlooked and by numerous findings of different groups that partially are in disagreement with each other. A large part of these discrepancies reflect the different methods of handling systematic errors. Evidently systematics are not yet under control or fully understood. We try to emphasize the importance to take these errors, in particular calibration issues, into account and put forward some measures adapted to the problem.
The bounds on the variation of μ are generally obtained by using the vibrorotational transitions of molecular hydrogen, since H_{2} is a very abundant molecule although very rarely seen in quasar absorbers. Only a few studies used other molecules since they are difficult to detect and measure accurately at large redshifts. In general these methods provide less stringent bounds on Δμ directly or bear a greater danger of nonuniform absorbers. Comparisons between the redshifts of H I 21 cm (hyperfine) measured in the radio regime and ultraviolet resonance dipole transitions are sensitive to changes in X ≡ g_{p}α^{2}/μ (see, i.e., Kanekar 2010a), which offers an important complementary verification of measured variations, although they sample different gas volumes.
One remarkable exception is the inverse spectrum of ammonia at radio wavelengths. A variation of Δμ/μ can be tested through precise measurements of the relative radial velocities of narrow molecular lines observed in the cold interstellar molecular cores. This approach is based on a new method derived by Flambaum & Kozlov (2007). Ammonia NH_{3} is a molecule whose inversion transitions are very sensitive to changes in μ due to a tunneling effect. The sensitivity coefficient of the inversion transition NH_{3}(1,1) at ν = 23.7 GHz is almost two orders of magnitude more sensitive to μvariation than H_{2} molecular rotational frequencies. By comparing the observed inversion frequency of NH_{3}(1, 1) with a suitable rotational frequency of another molecule arising cospatially with ammonia, a limit on the spatial variation of μ can be determined.
Ammonia has been detected in absorption in the main gravitational lenses of the quasars B 0218+357 and PKS 1830211. Flambaum & Kozlov (2007) combine the three detected NH_{3} absorption spectra from B0218+357 with rotational spectra of CO, HCO^{+}, and HCN to place a limit of (0.6 ± 1.9) × 10^{6} for a lookback time of 6 Gyr (redshift z = 0.68). Accounting in detail for the velocity structure of the line profiles, Murphy et al. (2008) reanalyzed the ammonia data in combination with newly obtained high signaltonoise rotational spectra of HCO^{+} and HCN. This yields <1.8 × 10^{6} at a 95% confidence level. Analyzing the ten NH_{3} inversion lines and a similar number of rotational transitions from other molecules Henkel et al. (2009) obtain 10^{6} as a firm upper limit for a lookback time of 7 Gyr (z = 0.89). However, the low number of NH_{3} sources limit this method considerably, in particular for high redshifts.
Radio observations of OH lines at the Arecibo Telescope and the Westerbork Synthesis Radio Telescope yield ΔG/G = (−1.18 ± 0.46) × 10^{5} for a look back time of 2.9 Gyr. G is defined as G ≡ g_{p} [μα^{2}] ^{1.85} and the results correspond to a change in α, μ and/or g_{p} (Kanekar et al. 2010b).Furthermore, the 21 cm radition is known to be sensitive to variations in α and can be utilized to set constraints on a possible variation at large redshifts z > 30 (Khatri & Wandelt 2007).
In the following we will concentrate on the single H_{2}system observed towards QSO 0347383 to trace the protontoelectron mass ration μ at high redshift (z_{abs} = 3.025). We intend to reach a robust estimation of the achievable accuracy with current data by comparing independent observation runs.
2. Data
2.1. Observations
Journal of the observations.
QSO 0347383 is a bright quasar (V ~ 17.3) with z_{em} 3.23, which shows a Damped Lyman α system at z_{abs} = 3.0245. The hydrogen column density is of N(H I) = 5 × 10^{20} cm^{2} with a rich absorptionline spectrum (Levshakov et al. 2002a). The z_{abs} = 3.025 DLA exhibits a multicomponent velocity structure. There are at least two gas components: a warm gas seen in lines of neutral atoms, H and low ions, and a hot gas where the resonance doublets of C IV and Si IV are formed. In correspondence of the cool component molecular hydrogen was first detected by Levshakov et al. (2002b) who identified 88 H_{2} lines.
All works on QSO 0347383 are based on the same UVES VLT observations^{3} in January 2002 (see Ivanchik et al. 2005). The data used therein were retrieved from the VLT archive along with the MIDAS based UVES pipline reduction procedures. The slit width was 0.8″. The grating angle for the QSO 0347383 observations had a central wavelength of 4300 Å. The images are 2 × 2 binned. The 9 spectra were recorded during 3 nights with an exposure time of 4500 s each. Additional observational parameters are described in Ivanchick et al. (2005). The above mentioned data was recently carefully reduced again by Thompson et al. (2009a).
Here we take into account additional observational data of QSO 0347383 acquired in 2002 at the same telescope but not previously analyzed^{4}.
The UVES observations comprised of 6 × 80 minexposures of QSO 0347383 on several nights, thus adding another 28.800 s of exposure time. The journal of these observations as well as additional information is reported in Table 1. Three UVES spectra were taken with the DIC1 and setting 390+580 nm and three spectra with DIC2 and setting 437+860, thus providing blue spectral ranges between 320–450 and 373–500 nm respectively. We note that QSO 0347–383 has no flux below 370 nm due to the Lyman discontinuity of the z_{abs} = 3.023 absorption system. The slit width was set to 1″ for all observations providing a Resolving Power of ~40 000. The different slit widths and hence different resolutions of the observation runs pose no problem since all data are analyzed separately during the fit. The seeing was varying in the range between 0.5″ to 1.4″ as measured by DIMM but generally is better than this at the telescope. The CCD pixels were binned by 2 × 2 providing an effective 0.027–0.030 Å pixel, or 2.25 km s^{1} at 400 nm along dispersion direction.
2.2. Reduction
The standard UVES pipeline has been followed for the data reduction. This includes sky subtraction and optimal extraction of the spectrum. Typical residuals of the wavelength calibrations were of ~0.5 mÅ or ~40 m s^{1} at 400 nm. The spectra were reduced to barycentric coordinates and air wavelengths have been transformed to vacuum by means of the dispersion formula by Edlen (1966). Proper calibration and data reduction will be the key to detailed analysis of potential variation of fundamental constants. The influence of calibration issues on the data quality is hard to measure and the magnitude of the resulting systematic error is under discussion. The measurements rely on detecting a pattern of small relative wavelength shifts between different transitions spread throughout the spectrum. Normally, quasar spectra are calibrated by comparison with spectra of a hollow cathode thorium lamp rich in unresolved spectral lines. However several factors are affecting the quality of the wavelength scale. The paths for ThAr light and quasar light through the spectrograph are not identical thus introducing small distortions between ThAr and quasar wavelength scales. In particular differences in the slit illuminations are not traced by the calibration lamp. Since source centering into the slit is varying from one exposure to another this induce an offset in the zero point of the scales of different frames which could be up to few hundred of m s^{1}. In Sect. 3.1 we provide an estimate of these offsets which result of a mean offset of 168 m s^{1} as well as a procedure to avoid this problem. Laboratory wavelengths are know with limited precision which is varying from line to line from about 15 m s^{1} of the better known lines to more than 100 m s^{1} for the more poorly known lines (Murphy et al. 2008; Thompson et al. 2009b). However, this is the error which is reflected in the size of the residuals of the wavelength calibration. Iodine cell based calibration cannot be applied directly in the case of QSO 0347383 since at a redshift of z ~ 3 all observed lines lie outside the range of Iodine lines which cover about 5000–6000 Å. Additionally, at the given level of continuum contamination due to Lymanα forest at such redshifts a superimposed spectrum of the iodine cell is not desirable.
Effects of this kind have been investigated at the Keck/HIRES spectrograph by comparing the ThAr wavelength scale with one established from I2cell observations of a bright quasar by Griest et al. (2010). They found both absolute and relative wavelength offsets in the Keck data reduction pipeline which can be as large as 500–1000 m s^{1} for the observed wavelength range. Such errors would correspond to Δλ ~ 10−20 m Å and exceed by one order of magnitude presently quoted errors (Thompson et al. 2009a). Very recently, Whitmore et al. (2010) estimate intraorder shifts of the UVES to reach up to 200 m s^{1}. Examination of the UVES spectrograph at the VLT carried out via solar spectra reflected on asteroids with known radial velocity showed no such dramatic offsets being less than ~100 m s^{1} (Molaro et al. 2008a) but systematic errors at the level of few hundred m s^{1} have been revealed also in the UVES data by comparison of relative shifts of lines with comparable response to changes of fundamental constants (Centurion et al. 2009). These examples well show that current Δμ/μanalysis based on quasar absorption spectra at the level of a few ppm enters the regime of calibration induced systematic errors. While awaiting a new generation of lasercombfrequency calibration, today’s efforts to investigate potential variation of fundamental physical constants require factual consideration of the strong systematics.
We note also that the additional observations considered here were taken for other purposes and the ThAr lamps are taken during daytime, which means several hours before the science exposures and likely under different thermal and pressure conditions. However, in the present work we bypass the possibility of different zero points of the different images via the seldom case of independent observations. Instead of coadding all the spectra we compute first the global velocity shifts between the spectra with the procedure described in the following section and we also utilize the whole uncertainties coming from the wavelength accuracies as part of the analysis procedure.
Fig. 1 Example region of the QSO 0347383 spectrum showing the recorded flux (dashed) and its interpolation via a polynomial using Neville’s algorithm to conserve the local flux. 
2.3. Noise level
The UVES data reduction procedure deliver the error spectrum along the optimally extracted spectrum. The given error in flux of all 15 spectra was tested against the zero level noise in saturated areas. A broad region of saturated absorption is available near 3906 Å in the observers frame. Statistical analysis revealed a variance corresponding to ~120% of the given error on average for the 15 spectra. This means that normally errors that rely to the standard extracted routine are probably underestimated by a comparable amount. In particular we compared the standard deviation of the flux between 3903.8 Å and 3908.7 Å (roughly 160 samples) with the average of the specified error for that range. In our analysis for each of the spectra the calculated correction factor was applied.
3. Preprocessing
3.1. Relative shifts of the 15 spectra
Prior to further data processing the reduced spectra are reviewed in detail. The first data set (henceforward referred to as set A) consists of nine separate spectra observed between 7th and 9th of January in 2002. The second set of 6 spectra (B) was obtained between January 13th and February 2nd in 2002 (see Table 1).
Due to slit illumination effects and grating motions the individual spectra are subject to small shifts – commonly on subpixel level – in wavelength. These shifts will be particularly crucial in the process of coaddition of several exposures. To estimate these shifts all spectra were interpolated by a polynomial using Neville’s algorithm to conserve the overall flux (see Fig. 1). The resulting pixel step on average is 1/20 of the original data. Each spectrum was compared to the others. For every data point in a spectrum the pixel with the closest wavelength was taken from a second spectrum. Their deviation in flux was divided by the quadratic mean of their given errors in flux. This procedure was carried out for all pixels inside certain selected wavelength intervals resulting in a mean deviation of two spectra. The second spectrum is then shifted against the first one in steps of ~1.5 mÅ. The run of the discrepancy of two spectra is of parabolic nature with a minimum at the relative shift with the best agreement. Figure 2 shows the resulting curve with a parabolic fit. In this exemplary case the second spectrum shows a shift of 6.2 mÅ in relation to the reference spectrum. The clean parabolic shape verifies the approach. Table 2 shows the corresponding offsets for the 15 spectra. The offsets between the exposures are relevant with a peak to peak excursion up to almost 800 m s^{1}. The average deviation is 2.3 mÅ or 170 m s^{1} at 400 nm. For further analysis in this paper all the 15 spectra are shifted to their common mean, which is taken as an arbitrary reference position. To avoid areas heavily influenced by cosmic events or areas close to overlapping orders only certain wavelength intervals were taken into account, namely the regions 3877–3886 Å, 3986–4027 Å, 4145–4175 Å and 4216–4240 Å (referred to as shift 1, 2, 3, 4 in Table 2). The global shift represents the obtained shift between two spectra measured in all four wavelength regions. The individual intervals show no significant differential shifts and their combined wavelength range was used to obtain a more robust mean shift between two spectra. The individual shifts for each wavelength region was merely obtained to estimate the error of the global shift given in Table 2. The routine was carried out for all spectrumcombinations and the resulting shifted spectra were checked for shifts again. We estimate the error per shift to be of 38 m s^{1} based on the deviation of the individual shifts of four wavelength intervals. Section 4.3 illustrates its influence on the data analysis with respect to the previous analysis of the data set A, in which this effect was not considered.
Fig. 2 Exemplary plot of the subpixel crosscorrelation. The resulting shift is ascertained via parabolic fit. In this case the two spectra are in best agreement with a relative shift of 6.2 ± 0.5 mÅ. 
Relative shifts of the observed spectra to their common mean.
3.2. Selection of lines and line fitting
The selection of suitable H_{2}features for the final analysis is rather subjective. As a matter of course all research groups crosschecked their choice of lines for unresolved blends or saturation effects. The decision whether a line was excluded due to continuum contamination or not, however, relied mainly on the expert knowledge of the researcher and was only partially reconfirmed by the ascertained uncertainty of the final fitting procedure. This work puts forward a more generic approach adapted to the fact that we have two distinct observations of the same object.
In this paper each H_{2}signature is fitted with a single component. The surrounding flux is fit by a ploynomial and the continuum is rectified accordingly. This approach is tested and verified in Wendt & Reimers (2008), however lines near saturated or steeply descending areas should be avoided. A selection of 52 (in comparison with 68 lines for that system by King et al. 2008) lines is fitted separately for each dataset of 9 (A) and 6 (B) exposures, respectively. In this selection merely blends readily identifiable or emerging from equivalent width analysis are excluded. Each rotational level is fitted with conjoined line parameters except for redshift naturally. A common column density N and broadening parameter b corresponds to each of the observed rotational levels (in this case J = 1,2,3).
The data are not coadded but analyzed simultaneously via the fitting procedure introduced in Quast et al. (2005). In principle each set of parameters (line centroid, broadening parameter, column density, coefficients of the continum polynomial) drawn from a large parameter space is tested in all individual spectra and judged by a weighted χ^{2}. The standard deviations of line positioning are provided by the diagonal elements of the scaled covariance matrix, a procedure described in detail in the above mentioned paper by Quast et al. and verified, i.e., in Wendt & Reimers (2008). For each of the 52 lines there are two resulting fitted redshifts or observed wavelengths, respectively, with their error estimates. To avoid false confidence, the single lines are not judged by their error estimate but by their difference in wavelength between the two data sets in relation to the combined error estimate. Figure 3 shows this dependency. The absolute offset Δλ_{effective} to each other is expressed in relation to their combined error given by the fit: (3)Figure 3 reveals notable discrepancies between the two datasets, the disagreement is partially exceeding the 5σ level^{5}. Since the fitting routine is known to provide proper error estimates (Quast et al. 2005; Wendt et al. 2008), the dominating source of error in the determination of line positions is due to systematic errors. This result indicates calibration issues of some significance at this level of precision. The comparison of two independent observation runs reveals a source of error that cannot be estimated by the statistical quality of the fit alone. For further analysis only lines that differ by less than 3σ are taken into account. This criterion is met by 36 lines. Figure 4 shows three examplary H_{2}features corresponding to the transitions L5R1, L5P1, L5R2. All have similar sensitivity towards changes in μ. L5P1 fails the applied self consistency check between the two data sets and is excluded in the further analysis. Table 4 lists the excluded lines.
Fig. 3 Selection of 52 apparently reasonable lines to be fitted separately for each dataset of 9 and 6 exposures, respectively. Their absolute offset Δλ_{effective} to each other is expressed in relation to their combined error given by the fit (see Eq. (3)). The dashed lines border the 3σ domain. 
Fig. 4 Part of the co added spectrum near 4176 Å. The data however, were not co added for the fit. L5R1 and L5R2 match the 3σ criterion, L5P1 does not. 
QSO 0347383 Line List.
It is noteworthy that line selections of this absorption system by other groups diverge from each other by a large amount. King et al. (2008) processed a total of 68 lines. By reconstructing the continuum flux with additionally fitted lines of atomic hydrogen they felt confident not to care about the relative position of the H_{2}features next to the Lymanα forrest. Fitting H_{2}features as single lines, however, is affected by the surrounding flux and its nature as simulations have shown (Wendt & Reimers 2008). Thompson et al. (2009a) selected 36 lines for analysis of which differs from our semiautomatical choice of lines by almost 40%.
Fig. 5 Final results in redshift vs. sensitivity coefficient K_{i} for this paper (circles), Ubachs et al. 2007 (squares) and Thompson et al. (2009a) (triangles). 
Hence, the different findings arise through in large parts independent analysis. Different approaches, line selections and in the end applied methods contribute to a more solid constraint on variation of fundamental constants. This variety is mandatory to understand contradicting findings, not only in case of the protontoelectron mass ratio. Table 3 report the molecular line position and relative errors. Figure 5 plots the results of this paper, Ubachs et al. (2007) and Thompson et al. (2009a), who published the individual fit parameters. The redshifts derived are of 3.0248969 (56), 3.0248988(29) and 3.0248987(61) for this paper, Ubachs et al. (2007) and Thompson (2009a) respectively, which is not surprising being based at least partially on the same data. All three analysis are based on the same source for sensitivity coefficients. The distribution of positioning errors for the mentioned works is illustrated in Fig. 6. The three sets of measure show a significant scatter around the mean quite in excess of the error in line position which is suggestive of the presence of systematic errors.
Fig. 6 Line positioning errors in km s^{1} for this paper (solid), Ubachs et al. (2007) (dashed) and Thompson et al. (2009a) (dotted), binned to 50 m s^{1}. 
Excluded lines.
The chosen Δλ criterium for line selection permits evaluation of the selfconsistency of a line positioning via fit for the involved data. While the availability of two independent observations on short time scale is rather special, it illustrates one applicable modality to avoid relying on the fitting apparatus alone.
4. Results
For the final analysis the selected 36 lines are fitted in all 15 shifted, errorscaled spectra simultaneously. The result of an unweighted linear fit corresponds to Δμ/μ = (15 ± 16) × 10^{6} over the lookback time of ~11.5 Gyr for z_{abs} = 3.025. Figure 7 shows the resulting plot. The complete list of lines is shown in Table 3. The approach to apply an unweighted fit is a consequence of the unknown nature of the prominent systematics. The observed scatter is in excess of the positioning errors. The fit to the data is not selfconsistent. For this work the calibration errors and the influence of unresolved blends are assumed to be dominant in comparison to individual fitting uncertainties per feature. For the following analysis the same error is adopted for each line. With an uncertainty in redshift of 1 × 10^{6} we obtain: Δμ/μ = (15 ± 6) × 10^{6}. However the goodnessoffit is below 1 ppm and is not self consistent. The goodness of fit of a statistical model describes how well it fits a set of observations. A linear model with the given parameters does not represent the observed data sample very well. The apparent discrepancies between model and data including their errorbars shown in Fig. 7 are extremely unlikely (below one part per million) to be chance fluctuations. Judging by that and Fig. 7, a reasonable error in observed redshift should at least be in the order of 4−5 × 10^{6}. The weighted fit gives: Δμ/μ = (15 ± 14) × 10^{6}.
This approach is motivated by the goodnessoffit test: Q(χ^{2}ν) is the probability that the observed chisquare will exceed the value χ^{2} by chance even for a correct model, ν is the number of degrees of freedom. Given in relation to the incomplete gamma function: (4)Assuming a Gaussian error distribution, Q gives a quantative measure or the goodnessoffit of the model. If Q ist very small for some particular data set, then the apparent discrepancies are unlikely to be chance fluctuations that would be expected for a Gaussian error distribution. Much more probably either the model is wrong or the size of the measurement errors is larger than stated. However, the chisquare probability Q does not directly measure the credibility of the assumption that the measurement errors are normally distributed. In general, models with Q < 0.001 can be considered inacceptable. In this case the model is given and hence the low probability is due to underestimated errors in the data. Solely for given errors of ~300 m s^{1}, corresponding to ~4 × 10^{6} in redshift for QSO 0347–383 the goodnessoffit parameter Q exceeds 0.001. The scale of the error appears to be ~300 m s^{1} to achieve a selfconsistent fit to the data.
Fig. 7 The unweighted fit for QSO 0347383 corresponds to Δμ/μ = (15 ± 16) × 10^{6}. The error bars correspond merely to the fitting uncertainty in the order of 180 m s^{1} on average. Note, that at such a high scatter z_{Ki = 0} differs from by less than 1σ_{z}. 
For the data on QSO 0347383 this corresponds to an error in the observed wavelength of roughly 4 m Å , which is notably larger than the estimated errors for the individual line fits which ranges from 0.5 m Å to 6.5 m Å with an average of 2.5 m Å (~180 m s^{1}). The systematic error contributes an uncertainty of about 2 m Å on average. The immediate calibration errors are in the order of 50 m s^{1} for set B and presumably slightly larger for set A. Figure 8 plots the data with errorbars corresponding to 180 m s^{1} and the total of 300 m s^{1}.
The final result can be subdivided as: Δμ/μ = (15 ± (9_{stat} + 6_{sys})) × 10^{6}. The comparably high scatter in Fig. 7 can partially be attributed to the approach to fit single H_{2}components with a polynomial fit to the continuum. In special cases, contaminated flux bordering a H_{2}signature can introduce additional uncertainty in positioning therefore checks for selfconsistency and systematics are of utmost importance.
The determination of the different errors involved is on a par with the actual result.
We believe that this result represents the limit of accuracy that can be reached with the given data set and the applied methods for analysis. The presented method yields a null result. The recent work by Thompson et al. (2009a) stated Δμ/μ = (−28 ± 16) × 10^{6} for a weighted fit based on the same system in QSO 0347383. The therein stated error reflects the statistical uncertainty alone.
Note, that the given systematics of 2.9 ppm for Keck/HIRES data given in Malec et al. (2010) are in first approximation estimated by the observed ~500 m s^{1} peaktopeak intraorder value reduced according to the number of molecular transitions observed, i.e. ~.
This work proposes to take alternative approaches into account when operating that close to the limits of several involved systems. The presented method was applied to the known QSO 0347383 data for two main reasons:

as an example to put forward alternative strategies;

a standalone determination of Δμ/μ based on QSO 0347383 to back up current nullresults and consequential constraints.
Fig. 8 Data identical to Fig. 7. The errorbars represent the average positioning error (solid) and the additional systematic error (dotted) of ~180 m s^{1} and ~120 m s^{1}, respectively. 
4.1. Uncertainties in the sensitivity coefficients
At the current level of precision, the influence of uncertainties in the sensitivity coefficients K_{i} is minimal. It will be of increasing importance though when wavelength calibration can be improved by pedantic demands on future observations. Eventually Laser Frequency Comb calibration will allow for practically arbitrary precision and uncertainties in the calculations of sensitivities will play a role. Commonly the weighted fits neglects the error in K_{i}.
Effective analysis in the future involves consideration of the error budget of the sensitivity coefficients. The χ^{2} merit function for the generic case of a straightline fit with errors in both coordinates is given by: (5)and can be solved numerically with valid approximations (Lybanon 1984).
At the current level even an error in K_{i} of about 10% merely has an impact on the error estimate in the order of a few 10^{6}, as resulted from simulations. The factual errors are expected to be in the order of merely a few percent (Ubachs et al. 2007), yet they might contribute to the precision of future analysis.
Alternatively the uncertainties in K_{i} can be translated into an uncertainty in redshift via the previously fitted slope: (6)The results of this ansatz are similar to the fit with errors in both coordinates and in general this is simpler to implement.
Another possibility is to apply a Gaussian error to each sensitivity coefficient and redo the normal fit multiple times with alternating variations in K_{i}. Again, the influence on the errorestimate is in the order of 1 ppm. The different approaches to the fit allow to estimate its overall robustness as well.
4.2. Individual line pairs
Δμ/μ can also be obtained by using merely two lines that show different sensitivity towards changes in the protontoelectron mass ratio. Another criterion is their separation in the wavelength frame to avoid pairs of lines from different ends of the spectrum and hence in particular errorprone. Several tests showed that a separation of Δλ ≤ 110 Å and a range of sensitivity coefficients K_{1} − K_{2} ≥ 0.02 produces stable results that do not change any further with more stringent criteria. Pairs that cross two neighboring orders (~50 Å) show no striking deviations either. Figure 9 shows the different values for Δμ/μ derived from 52 line pairs that match the aforementioned criteria. Note, that a single observed line contributes to multiple pairs. The gain in statistical significance by this sorting is limited as pointed out by Molaro et al. (2008b). Their average value yields Δμ/μ = 6 ± 12 × 10^{6}. The scatter is then related to uncertainties in the wavelength determination which is mostly due to calibration errors. The standard error is 8 × 10^{6}.
The approach to use each observed line only once in the analysis is plotted in Fig. 9 as filled squares. The pairs to derive Δμ/μ from were constructed by grouping the line with the highest sensitivity value together with the line corresponding to the lowest value for K_{i} and so on with the remaining lines. The distance in wavelength space between the two lines was no critierum and it ranges from 20 Å to 590 Å (see Table 5). Without reutilization of lines, 11 pairs with a coverage in sensitivity of ΔK_{i} ≥ 0.02 were found.
Evidently the usage of lines with comparably large distances in the spectrum has no influence on the results.
Grouping all observed lines into 17 pairs of maximum K_{i} sensitivity not considering their separation in wavelength space (rightmost column).
Fig. 9 Δμ/μ derived from individual line pairs (52) which are separated by less than 110 Å and show a difference in sensitivity of more then 0.02. The errorbars reflect the combined positioning error of the two contributing lines. The weighted fit corresponds to Δμ/μ = (6 ± 12) × 10^{6}. The filled squares graph 11 line pairs, selected to give the largest difference in sensitivity (≥ 0.02) towards variation in μ (see Table 5). 
Fig. 10 Variation in fitted positions for all lines with and without initial correction for shifts in between the 15 spectra. The slope of the fit is dominated by three lines. 
4.3. Influence of the preprocessing
Section 3.1 describes the initial shift to a common mean of all 15 spectra. The complete analysis was redone with errorscaled
but unshifted spectra and the ascertained line positions of both runs compared. Figure 10 shows the difference for each H_{2}line in mÅ over the corresponding sensitivity coefficients K_{i}. The plotted line is a straight fit. Clearly the slope is dominated by three individual lines whose fitted centroids shifted up to 5.5 mÅ due to the preprocessing. These three lines in particular produce a trend towards variation in μ when grating shifts and other effects are not taken into account. This singlesided trend probably occurred by mere chance but at such low statistics it influences the final result. Similar effects might have introduced trends of nonzero variation in former works (i.e., Ivanchik et al. 2005; Reinhold et al. 2006).
Lines fitted with seemingly high precision and thus a low error reach higher offsets than lines with a larger estimated error at the same discrepancy in λ_{obs}. Clearly the lower error estimates merely reflects the statistical quality of the fit, not the true value of the specific line position.
Acknowledgments
We are thankful for the support from the Collaborative Research Centre 676 and for helpful discussions on this topic with D. Reimers, S. A. Levshakov, P. Petitjean and M. G. Kozlov.
References
 Blatt, S., Ludlow, A. D., Campbell, G. K., et al. 2008, Phys. Rev. Lett., 100, 14 [Google Scholar]
 Centurión, M., Molaro, P., & Levshakov, S. 2009, [arXiv:0910.4842] [Google Scholar]
 Edlén, B. 1966, Metrologia, 2, 71 [NASA ADS] [CrossRef] [Google Scholar]
 Flambaum, V. V., & Kozlov, M. G. 2007, Phys. Rev. Lett., 98, 24 [Google Scholar]
 Fritzsch, H. 2009, Physics Uspekhi, 52, 359 [Google Scholar]
 Griest, K., Whitmore, J. B., Wolfe, A. M., et al. 2010, ApJ, 708, 158 [NASA ADS] [CrossRef] [Google Scholar]
 Ivanchik, A., Petitjean, P., Varshalovich, D., et al. 2005, ApJ, 440, 45 [Google Scholar]
 Kanekar, N., Chengalur, J. N., & Ghosh, T. 2010a, ApJ, 716, 23 [NASA ADS] [CrossRef] [Google Scholar]
 Kanekar, N., Prochaska, J. X., Ellison, S. L., & Chengalur, J. N. 2010b, ApJ, 712, 148 [Google Scholar]
 Khatri, R., & Wandelt, B. D. 2007, Phys. Rev. Lett., 98, 11 [Google Scholar]
 King, J. A., Webb, J. K., Murphy, M. T., & Carswell, R. F. 2008, Phys. Rev. Lett., 101 [Google Scholar]
 Levshakov, S. A., DessaugesZavadsky, M., D’Odorico, S., & Molaro, P. 2002a, MNRAS, 333, 373 [NASA ADS] [CrossRef] [Google Scholar]
 Levshakov, S. A., DessaugesZavadsky, M., D’Odorico, S., & Molaro, P. 2002b, ApJ, 565, 696 [NASA ADS] [CrossRef] [Google Scholar]
 Lybanon, M. 1984, AJP, 52, 22 [Google Scholar]
 Mohr, P. J., & Taylor, B. N. 2000, Rev. Mod. Phys., 72, 351 [NASA ADS] [CrossRef] [Google Scholar]
 Malec, A. L., Buning, R., Murphy, M., et al. 2010, MNRAS, 403, 1541 [NASA ADS] [CrossRef] [Google Scholar]
 Molaro, P., Levshakov, S. A., Monai, S., et al. 2008a, A&A, 481, 559 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Molaro, P., Reimers, D., Agafonova, I. I., & Levshakov, S. A. 2008b, EPJ, 163, 173 [Google Scholar]
 Murphy, M. T., Webb, J. K., Flambaum, V. V., et al. 2008b, MNRAS, 384, 1053 [NASA ADS] [CrossRef] [Google Scholar]
 Quast, R., Baade, R., & Reimers, D. 2005, ApJ, 431, 1167 [Google Scholar]
 Reinhold, E., Buning, R., Hollenstein, U., et al. 2006, Phys. Rev. Lett., 96, 15 [Google Scholar]
 Thompson, R. I. 1975, Astrophys. Lett., 16, 3 [Google Scholar]
 Thompson, R. I., Bechtold, J., Black, J. H., et al. 2009a, ApJ, 703, 2 [Google Scholar]
 Thompson, R. I., Bechtold, J., Black, J. H., & Martins, C. J. A. P. 2009b, New A, 14, 379 [Google Scholar]
 Ubachs, W., Buning, R., Eikema, K. S. E., & Reinhold, E. 2007, J. Molec. Spec., 241, 155 [Google Scholar]
 Wendt, M., & Reimers, D. 2008, EPJ, 163, 197 [Google Scholar]
 Whitmore, J. B., Murphy, M. T., & Griest, K. 2010, ApJ, 723, 89 [NASA ADS] [CrossRef] [Google Scholar]
All Tables
Grouping all observed lines into 17 pairs of maximum K_{i} sensitivity not considering their separation in wavelength space (rightmost column).
All Figures
Fig. 1 Example region of the QSO 0347383 spectrum showing the recorded flux (dashed) and its interpolation via a polynomial using Neville’s algorithm to conserve the local flux. 

In the text 
Fig. 2 Exemplary plot of the subpixel crosscorrelation. The resulting shift is ascertained via parabolic fit. In this case the two spectra are in best agreement with a relative shift of 6.2 ± 0.5 mÅ. 

In the text 
Fig. 3 Selection of 52 apparently reasonable lines to be fitted separately for each dataset of 9 and 6 exposures, respectively. Their absolute offset Δλ_{effective} to each other is expressed in relation to their combined error given by the fit (see Eq. (3)). The dashed lines border the 3σ domain. 

In the text 
Fig. 4 Part of the co added spectrum near 4176 Å. The data however, were not co added for the fit. L5R1 and L5R2 match the 3σ criterion, L5P1 does not. 

In the text 
Fig. 5 Final results in redshift vs. sensitivity coefficient K_{i} for this paper (circles), Ubachs et al. 2007 (squares) and Thompson et al. (2009a) (triangles). 

In the text 
Fig. 6 Line positioning errors in km s^{1} for this paper (solid), Ubachs et al. (2007) (dashed) and Thompson et al. (2009a) (dotted), binned to 50 m s^{1}. 

In the text 
Fig. 7 The unweighted fit for QSO 0347383 corresponds to Δμ/μ = (15 ± 16) × 10^{6}. The error bars correspond merely to the fitting uncertainty in the order of 180 m s^{1} on average. Note, that at such a high scatter z_{Ki = 0} differs from by less than 1σ_{z}. 

In the text 
Fig. 8 Data identical to Fig. 7. The errorbars represent the average positioning error (solid) and the additional systematic error (dotted) of ~180 m s^{1} and ~120 m s^{1}, respectively. 

In the text 
Fig. 9 Δμ/μ derived from individual line pairs (52) which are separated by less than 110 Å and show a difference in sensitivity of more then 0.02. The errorbars reflect the combined positioning error of the two contributing lines. The weighted fit corresponds to Δμ/μ = (6 ± 12) × 10^{6}. The filled squares graph 11 line pairs, selected to give the largest difference in sensitivity (≥ 0.02) towards variation in μ (see Table 5). 

In the text 
Fig. 10 Variation in fitted positions for all lines with and without initial correction for shifts in between the 15 spectra. The slope of the fit is dominated by three lines. 

In the text 
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