Nonlinear corrections to the cosmological matter power spectrum and scale-dependent galaxy bias: implications for parameter estimation
We explore and compare the performances of two nonlinear correction and scale-dependent biasing models for the extraction of cosmological information from galaxy power spectrum data, especially in the context of beyond-CDM cosmologies. The first model is the well known model, first applied in the analysis of 2dFGRS data. The second, the model, is inspired by the halo model, in which nonlinear evolution and scale-dependent biasing are encapsulated in a single non-Poisson shot noise term. We find that while both models perform equally well in providing adequate correction for a range of galaxy clustering data in standard CDM cosmology and in extensions with massive neutrinos, the model can give unphysical results in cosmologies containing a subdominant free-streaming dark matter whose temperature depends on the particle mass, e.g., relic thermal axions, unless a suitable prior is imposed on the correction parameter. This last case also exposes the danger of analytic marginalisation, a technique sometimes used in the marginalisation of nuisance parameters. In contrast, the model suffers no undesirable effects, and is the recommended nonlinear correction model also because of its physical transparency.
The past decade saw an explosion of precision cosmological measurements. Foremost amongst these is the observation of temperature and polarisation fluctuations in the cosmic microwave background (CMB) by a range of experiments [1, 2, 3, 4, 5, 6]. The distribution of large-scale structures (LSS) has also been mapped to unprecedented breadths and depths by galaxy redshift surveys such as the Two-Degree Field Galaxy Redshift Survey (2dFGRS)  and the Sloan Digital Sky Survey (SDSS) [8, 9]. Together with observations of distant type Ia supernovae [10, 11], these measurements have fostered the emergence of a benchmark framework—the adiabatic, nearly scale-invariant, “vanilla” CDM model—based on which one can test for evidence of new physics.
Clustering statistics of galaxies as probed by surveys like 2dF and SDSS are particularly well suited for the exploration of physics that introduce new effects on length scales . A classic example is the possibility to detect a subdominant component of free-streaming hot dark matter (HDM) , notably massive neutrinos [13, 14] and variants such as thermal axions [15, 16, 17, 18, 19], light gravitinos , et cetera. The sensitivity of these surveys at small length scales also lends a greater lever arm to the search for features in the primordial density perturbation power spectrum, possible remnants of inflationary physics [21, 22]. Last but not least, since the power spectrum of large-scale structures probes uniquely the parameter combination , it helps to lift the degeneracy between—and hence tighten the constraints on—the physical matter density and the Hubble parameter from CMB observations alone.
Usage of data from galaxy clustering surveys is based on the premise that one can reliably predict the distribution of galaxies, at least on a statistical basis, from theory. This is complicated by a number of factors. First, galaxies are necessarily collapsed objects, i.e., they have undergone a phase of nonlinear evolution. Using them as tracers of the underlying matter field implicitly assumes we know how to relate the two distributions to one another. A reasonable assumption is that on sufficiently large scales the power spectra of galaxies and of the matter field are identical up to a constant normalisation, or bias, factor. But this bias relation is expected to become scale-dependent when the dimesionless power spectrum of the galaxies exceeds unity [23, 24]. Indeed, the apparent tension between the 2dF and the SDSS galaxy power spectra is now believed to have originated from a more strongly scale-dependent bias factor for the red galaxies dominating the SDSS galaxy catalogue [25, 26]. On the theoretical front, a good deal of recent effort has also been devoted to understanding the origin of scale-dependent biasing (e.g., [27, 28]).
Second, galaxy positions are inferred from their redshifts. However, the peculiar motions of the galaxies, particularly when amplified by virialisation, induce additional Doppler shifts that can potentially obscure the inference. This is known as redshift space distortion, and on small length scales requires corrections beyond linear perturbation theory. Third, the clustering of the underlying dark matter field itself becomes nonlinear on scales . Thus, how reliably one can extract cosmological information from galaxy clustering statistics depends crucially on how well one can model these three nonlinear effects.
While all three effects can in principle be modelled by numerical simulations, these simulations, and indeed our understanding of galaxy formation, are not yet at a stage where one can reliably predict the power spectrum of galaxies as a function of galaxy type and redshift given some underlying cosmological model. In the meantime, nonlinear evolution and scale-dependent biasing must be modelled empirically as a systematic effect and the associated nuisance parameters marginalised when extracting cosmological information from galaxy clustering surveys, especially in beyond-CDM cosmologies.
In this connection, Cole et al.  recently proposed a correction formula which maps directly between the matter power spectrum calculated from linear perturbation theory and the power spectrum expected for the galaxies ,
The formula is partially calibrated against CDM-based semi-analytic galaxy formation simulations ( for redshift space, and for real space), and contains two free parameters ( and ) to be fixed by observational data. Equation (1.1) has been applied to the galaxy power spectra of 2dF  and the SDSS luminous red galaxy (LRG) sample  to test standard vanilla cosmology. However, there is a priori no guarantee that its usefulness extends also to cosmologies beyond CDM. Indeed, as we shall show below, equation (1.1) can be highly pathological when applied to certain classes of cosmological models containing a subdominant component of free-streaming dark matter.
In comparison, a conceptually more appealing framework in which to discuss nonlinear corrections is the halo model [29, 30, 31, 32]. Building on the assumptions of (i) hierarchical clustering, and (ii) that galaxies form only inside dark matter halos, halo model-based nonlinear corrections can in principle be made applicable to all hierarchical CDM cosmologies. The minimal model proposed in references [35, 33, 34], for example,
where and are free parameters, does not demand vanilla CDM as the sole input cosmology.
In the present work, we explore and compare the performance of these nonlinear correction models in some detail. We confront them with various observed galaxy power spectra, especially in the context of beyond-CDM cosmologies. We discuss parameter degeneracies and the role of priors on the nuisance parameters.
The paper is organised as follows. We describe first in section 2 the galaxy clustering data sets used in the analysis. Section 3 contains a more detailed discussion of the two nonlinear models we wish to explore. In sections 4, 5 and 6 we test the nonlinear models against data for standard vanilla cosmology, vanilla with massive neutrinos, and vanilla with thermal axions respectively. We conclude in section 7.
2 Data sets
We use the publicly available galaxy power spectra from the following galaxy catalogues.
This data set comes from the final data release of the Two-Degree Field Galaxy Redshift Survey . We use up to 36 data bands, corresponding to redshift space power spectrum data for wavenumbers .
Real space power spectrum of the main galaxy sample from the Sloan Digital Sky Survey data release 2 . We use up to 19 data bands, i.e., .
Real space power spectrum of the luminous red galaxies from the Sloan Digital Sky Survey data release 4 . The 20 data bands correspond to wavenumbers .
We also use at times CMB data from the Wilkinson Microwave Anisotropy Probe experiment after three years of observations [37, 38, 39], mainly for the construction of priors on certain cosmological parameters. This calculation is performed using version 2 of the likelihood package provided by the WMAP team on the LAMBDA web page .
3 Two nonlinear models
3.1 The model
We refer to the correction formula (1.1) as the model.
For CDM cosmologies, galaxy formation simulations suggest
that the parameter can be held fixed at in redshift space and at in real space .
The parameter , however,
exhibits a strong dependence on the galaxy type. Fitting the
model to the 2dF galaxy power spectrum at , Cole et al. found
for vanilla cosmology . Tegmark et
al.  applied the same model to SDSS-4 LRG, for
which provides a good fit.
Note that the case of is not equivalent to no nonlinear correction, since a nonzero parameter also modulates the power spectrum in a scale-dependent way. For , the model suppresses the power spectrum at . However, for values as large as such as required by the SDSS-4 LRG, the main role of the model is to add power at .
3.2 The model
The functional form of the model (1.1) was recently criticised in reference  for its incorrect dependence on . Specifically, it lacks a constant term to account for the presence of non-Poisson shot noise, a generic consequence of the assumption that galaxies form exclusively in halos. Indeed, from the halo model [29, 30, 31, 32], one should expect a correction formula with the skeletal form,
Here, the two-halo term, , arises from correlations between galaxies in two different halos, and approximates the familiar linear bias relation on large scales,
The one-halo term
accounts for correlations within the same halo and is approximately independent of the exact spatial distribution of the galaxies within a halo provided is not too large. Combining equations (3.2) and (3.3) we recover the minimal model (1.2).
The role of the shot noise term is to add power at small length scales, so that the ratio is effectively scale-dependent at large values. This is in contrast with the model (1.1), which for some values of the nonlinear parameter suppresses the power spectrum on the observable scales. Interestingly, taken at face value, the model also predicts a significant -dependence for as when once again rises above . It should be noted however that this small- behaviour is not present for dark matter clustering, since momentum conservation demands that the dark matter power spectrum falls off faster than as , a behaviour also observed in numerical simulations [42, 43]. On the other hand, a non-vanishing shot noise on large scales is in principle not forbidden for galaxy clustering, since tracers need not conserve momentum. Whether or not this is so remains to be understood.
In the present work we take the view that since galaxy clustering has not been observed on scales where the shot noise behaviour may become problematic (), equation (1.2) constitutes a sufficient phenomenological model to describe the galaxy power spectrum at .
Additional modifications to the basic model (1.2) to account for the damping of baryon acoustic oscillations and other nonlinear mode coupling effects have been discussed in the literature [28, 43, 44, 45]. These generally lead to nonlinear models of the form
where is some function of that depends also on the galaxy type. It is also possible to extend the halo model to include redshift space distortion [35, 45, 46]. We ignore these additional corrections in the present analysis in order to keep the number of extra fit parameters to a minimum. However, we emphasise that the effects encapsulated by will become increasingly important as more precise data from future galaxy redshift surveys become available.
4 Test 1: vanilla
To compare the performance of the two nonlinear models, we test them against galaxy clustering data in three minimal parameter spaces:
We take the geometry of the universe to be flat, and the initial conditions adiabatic. The parameter accounts for the normalisation of the galaxy power spectrum, and incorporates both the amplitude of the primordial scalar perturbations and the constant galaxy bias factor . We do not use any nonlinear correction for parameter space (i), i.e., . For parameter spaces (ii) and (iii), we use the model (1.2) and the model (1.1) respectively.
Note the definition of the matter density parameter . We choose this parameterisation because the turning point of the matter power spectrum is sensitive to the comoving Hubble radius at matter–radiation equality, which, for fixed values of , depends on , not the physical matter density . For fixed values of and , alone determines the broad shape of the matter power spectrum within the CDM framework.
We use standard Bayesian inference techniques and the Markov Chain Monte Carlo package CosmoMC [47, 48] to explore the posterior hypersurfaces as functions of the model parameters and the galaxy clustering data sets of section 2. Here, we note that within the vanilla framework, the physical baryon density , the Hubble parameter , and the scalar spectral index can be individually well constrained by CMB observations. This information is encapsulated in a set of “WMAP-3 priors” in table 1, which we apply when varying these three parameters. This approach differs slightly from the more common practice of fixing the parameter values and adopted in, e.g., references [7, 26]. Reference  further fixes . Our approach has the advantage that it properly takes into account the uncertainties on these parameters and thus avoids two inherent dangers of fixed parameter analyses: biased parameter estimates and underestimated errors. Additionally, it permits a consistent comparison of our constraints not only between different galaxy clustering data sets, but also with those obtained from CMB observations alone.
Broad, top-hat priors are imposed on the remaining parameters (table 1). For the parameter , we choose the range 0–50 for all three data sets. In the absence of additional information from, e.g., galaxy formation simulations, the upper limit of this prior is somewhat arbitrary. We will discuss this point in more detail in section 6. For the prior, the upper limit denotes the minimum clustering power measured by a survey. In other words, the linear matter power spectrum must not be negative anywhere. For 2dF, SDSS-2 main, and SDSS-4 LRG, , respectively.
4.2 The internal test: do the individual data sets call for nonlinear correction?
Figures 1 to 3 show the 1D marginal constraints on the parameters and the corresponding minimum and numbers of degrees of freedom (d.o.f.) as functions of the maximum wavenumber included in the analysis. The number of d.o.f. is defined here as the number of data points plus the number of priors, minus the number of fit parameters; its actual value might be slightly lower, because the power spectrum data points are not completely uncorrelated owing to overlapping window functions.
For , the green/shaded regions correspond to the 1D marginal 68% minimum credible intervals (MCI), while the 1D modes are indicated by black/dotted lines. On the other hand, the marginalised posterior distributions in and are often extremely flat, especially at small values of . While it is technically possible to construct credible intervals in these cases, quoting such an interval would distract from the fact that the parameters are essentially unconstrained. Therefore, instead of Bayesian intervals, we give in figures 1 to 3 for and the parameter regions satisfying
where is the 1D marginal posterior and denotes its value at the 1D mode. We loosely label this the “” interval. For large values, especially , where the posterior distributions are approximately Gaussian, this interval is identical to the 68% MCIs. See reference  for more detailed discussions of the various statistical quantities.
Changes in the estimates
The effects of nonlinear correction are most evident when we include data beyond . Here, nonlinear correction generally shifts the estimates to lower values relative to the case with no correction, irrespective of the nonlinear model used. For SDSS-4 LRG, this shift is very dramatic: at the 68% MCI moves down by an amount comparable to six or seven times its half-width (figure 1). In contrast, the shifts induced for 2dF and SDSS-2 main by either nonlinear model are mild: at a small overlap between the 68% MCIs before and after correction can still be seen in figures 3 and 3.
The need for nonlinear correction in the case of SDSS-4 LRG is corroborated by a comparison of the minimum values. Between correction and no correction, figure 1 shows that at , changes from for 18 d.o.f. to for 17 d.o.f., again irrespective of the nonlinear model used. On the other hand, similar comparisons for 2dF and for SDSS-2 main in figures 3 and 3 do not indicate any urgent need for an extra correction parameter: for 2dF, ; for SDSS-2 main, is virtually negligible.
We consider a data set internally consistent if the credible intervals agree for all choices of . For SDSS-4 LRG, figure 1 clearly demonstrates that nonlinear correction is necessary in order to achieve some semblance of internal consistency. A small discrepancy remains after correction: at and the 68% MCIs do not quite touch each other. However, this discrepancy is not statistically significant. We bring up this point here nonetheless as a cautionary note against over-interpretion of credible intervals.
How much correction?
Focussing on the cases with nonlinear correction, we see in figures 1 to 3 that while SDSS-4 LRG clearly prefers a nonzero correction parameter—be it or —at , the 2dF and the SDSS-2 main data sets do not exhibit the same strong preference. For SDSS-2 main and most choices of for 2dF, the regions include and (although, as mentioned before, the case of is not equivalent to no nonlinear correction). At , the parameters and cannot be constrained by data.
In terms of the model, roughly half of the small scale () power in SDSS-4 LRG can be attributed to the shot noise term. For 2dF and SDSS-2 main, the shot noise contribution is about a quarter according to the 1D mode.
Which nonlinear model?
Perhaps the most striking feature about the two nonlinear models considered here is that their corrective effects appear to be identical. This is particularly apparent in figures 1 and 3 at , where the preferred values of the correction parameters and exhibit virtually the same dependence on . At the estimates also show little if any dependence on the priors imposed on the nonlinear correction parameters. Thus as far as vanilla cosmology is concerned, there is no preference for either nonlinear model from a phenomenological standpoint, although the transparency of the model still makes it the more attractive one of the two.
4.3 The external test: are all data sets consistent with each other?
Figure 4 shows how the constraints on obtained from different galaxy clustering data sets and with different nonlinear correction methods compare with each other. For good comparison we indicate in the figure also the corresponding estimate from WMAP-3. Similar information is available in table 2, in which we give the 1D marginal 68% and 95% MCIs at ( for 2dF).
|Data set||No correction||model||model|
|SDSS-4 LRG||0.234–0.252 (0.227–0.262)||0.163–0.184 (0.153–0.195)||0.169–0.191 (0.158–0.202)|
|2dF||0.167–0.204(0.152–0.228)||0.134–0.173 (0.122–0.196)||0.134–0.178 (0.118–0.207)|
|SDSS-2 main||0.233–0.277 (0.213–0.300)||0.190–0.250 (0.167–0.279)||0.193–0.276 (0.167–0.316)|
|SDSS-4 LRG||–||3980–5170 (3380–5740)||22.7–25.5 (18.6–37.9)|
|2dF||–||452–1310 ()||7.0–19.2 (2.5–27.3)|
For both SDSS-4 LRG and SDSS-2 main, nonlinear correction clearly leads to better agreement with 2dF and with WMAP-3 at . In the case of SDSS-2 main, although the correction is not sufficient to cause the 68% region to overlap with that from 2dF (using the same correction method), the two 95% regions are certainly consistent. Importantly, the level of disagreement between SDSS-2 main and 2dF after correction is no worse than the small internal inconsistency between the low and the high constraints on from SDSS-4 LRG already discussed in section 4.2. Thus if we should accept that the nonlinear models (1.1) and (1.2) offer sufficient correction for SDSS-4 LRG, logically we must also consider them adequate for SDSS-2 main.
Lastly, we observe in figure 4 that the 2dF preferred values of tend in any case to be on the low side of SDSS-2 main, even at values of well below those at which nonlinearity nominally sets in. This suggests that the residual inconsistency after nonlinear correction can rather be put down to a statistical aberration at small values, than is indicative of a failure of either nonlinear model. Indeed, Sanchez and Cole  compared directly the power spectra of red galaxies (believed to be the main source of scale-dependent biasing) from 2dF and the main galaxy sample of SDSS data release 5, and found a similar discrepancy in the raw power spectrum data (see figure 7 of their paper). Our SDSS-2 main data set is but a subsample of SDSS data release 5; that it contains the same small fluctuation should be of no surprise.
5 Test 2: vanilla+massive neutrinos
It is well known that a subdominant component of massive neutrino HDM in the matter content slows down the growth of density perturbations on small length scales. In terms of the matter power spectrum, we expect a suppression of power of order at , where is the neutrinos’ free-streaming wavenumber, and the neutrino energy density. Since this suppression effectively changes the shape of the matter power spectrum at large wavenumbers, some amount of degeneracy could conceivably exist between the neutrino energy density and the nonlinear correction parameters. In this section we investigate the possible existence of such a degeneracy, and if so, its effects on massive neutrino cosmology.
We consider three parameter spaces:
Here, the neutrino fraction is defined as the ratio of the neutrino energy density to the total matter density . The former is given by the well known expression
where denotes the sum of the neutrino masses. We assume 3.04 degenerate neutrino species, which should be a good approximation since neither CMB nor galaxy clustering measurements are at present sufficiently sensitive to , where one might expect some small effects due to the neutrino mass hierarchy.
We fit these three cases to SDSS-4 LRG up to , using no nonlinear correction in case (i), and correction with the and the model respectively for cases (ii) and (iii). As in the previous section, we impose WMAP-3 priors on the parameters , , and tabulated in table 1. Note that these priors differ from those used previously, since CMB constraints are model-dependent. We adopt a top-hat prior on , 0–0.5, while for we use 0–100, in anticipation that more nonlinear correction may be required to offset the higher values usually inferred in cosmologies with massive neutrinos.
5.2 Results and discussions
Table 3 shows the 1D 68% and 95% MCIs for , , and the nonlinear parameters and for the three cases considered. We also give the minimum values as a measure of the goodness-of-fit.
|No correction||0.246–0.287 (0.232–0.314)||0.01–0.047 ()||–||63.2|
|model||0.168–0.216 (0.154–0.256)||()||4070–5270 (3430–5810)||19.7|
|model||0.171–0.226 (0.158–0.274)||()||23.6–36.9 (17.5–47.5)||20.6|
As in the case for vanilla cosmology, fitting the SDSS-4 LRG data without nonlinear correction leads to a very poor goodness-of-fit; the value is 63.2, for approximately degrees of freedom (20 data points of SDSS-4 LRG, 3 for the priors on , and , and for 6 free parameters). Adding nonlinear correction reduces by more than 40 units at the expense of only one extra parameter. Again, both nonlinear models offer very similar corrections to the power spectrum in terms of the inferred and values, although the model appears to provide a slightly better fit to the data judging by its slightly smaller . Interestingly, despite the dramatic decrease in the minimum between correction and no correction, the resulting shifts in the and estimates are deceptively small so that the 95% MCIs remain compatible before and after correction.
In the absence of nonlinear correction, the 95% upper limit on is about a factor of two too tight compared with the corrected case. This situation is reminiscent of the overly constraining bounds on derived in some recent combined analyses of WMAP-3 and the flux power spectrum of the Lyman- forest . Too much power at large wavenumbers—either because of uncorrected nonlinearities in the galaxy power spectrum or an unusually large normalisation in the case of the Lyman- forest—leads to the appearance of an overly flat matter power spectrum, which in turn prefers a smaller neutrino fraction and hence a smaller neutrino mass. The difference between the two corrected bounds is about 20%. The corresponding 95% limits on , for the model and for the model, differ by even less. Thus cosmological neutrino mass determination is at present unaffected by our choice of nonlinear correction model.
Finally, we see in figure 5 that no strong degeneracy exists between the neutrino fraction and the nonlinear correction parameters and . For small values of , the changes induced in the linear matter power spectrum by massive neutrino dark matter can be approximately mimicked by a redefinition of the apparent parameter ,
assuming . Here, is the parameter that is actually constrained by power spectrum data, while denotes the true value of . This expression also encapsulates the well known (approximate) degeneracy between and . Larger values induce more complicated changes in the power spectrum, and it is reassuring to see that these changes are not degenerate with nonlinear correction using either model.
6 The pathology of the model: vanilla+thermal axions
While both nonlinear models work very well for vanilla and for vanilla+massive neutrino cosmologies, and we may be tempted to conclude that they are for all purposes phenomenologically identical, we provide in this section a counter-example in which the incorrect functional form of the model can lead to some misleading results.
The case in point is a class of models containing a possible subdominant HDM component due to relic thermal axions with mass . These models differ from those with massive neutrino HDM in that the temperature and hence the number density of the axions are functions of , since determines when the particle species should decouple from the primordial plasma. Here, the function denotes the effective number of thermal degrees of freedom at the time of decoupling, and must be calculated by carefully tracking the freeze-out process (e.g., ).
Thus, although qualitatively thermal axion HDM exhibits free-streaming features very similar to those of massive neutrinos, quantitatively the suppression of small scale power in the matter power spectrum has a nonlinear dependence on the axion mass. We show in this section how this nontrivial dependence can cause some problems for the model.
We consider three parameter spaces:
, with a top-hat prior 0–100 on ,
, with a top-hat prior 0–200 on , and
Cases (i) and (ii) both use the nonlinear model (1.1), and differ only in the priors imposed on the correction parameter . Case (iii) uses the nonlinear model (1.2), with the usual prior on (see table 1). We fit each case to the combined data set WMAP-3+SDSS-4 LRG, using data up to for the latter.
6.2 Results and discussions
Figure 6 shows the 2D marginal 68% and 95% MCIs for , , and , as well as the 1D marginal posteriors for the the same three parameters for cases (i) and (ii).
Consider first the 1D marginal posteriors for . We see in figure 6 that the posteriors in both cases (i) and (ii) remain finite all the way up to the upper limit of the prior imposed on . This is also reflected in the relevant 2D contours, which are abruptly cut off at and respectively. Data alone does not constrain in this class of cosmological models.
While this does not affect the estimates, the inference of the axion mass depends crucially on how well we can constrain because of a persisting degeneracy between the two parameters. Indeed, if we do not cut off by hand at some sufficiently small value, a second peak begins to appear in the posterior at , besides the one at . From figure 7 we see that the power spectra for the two peaks after nonlinear correction are almost perfectly degenerate up to (and beyond) , even though the corresponding linear matter power spectra differ markedly already at .
We may be inclined to regard a 6 eV axion and, by implication, a large value as unphysical because the former runs in conflict with constraints on derived from stellar energy loss arguments and from telescope searches for axion radiative decays . Furthermore, the -degeneracy exists only in a limited range: as shown in figure 7, the corrected power spectra for the two peaks begin to deviate at . This suggests that the exact location of the high peak in -space may in fact depend on our choice of . Naturally we could have avoided this second peak simply by demanding consistency with other astrophysical constraints on . However, in the absence of, e.g., galaxy formation simulations for this very class of cosmological models, we have a priori no reason to reject or any other higher or lower value besides our own prejudices. Moreover, even if we manage to avoid the second peak with a finely tuned prior on , the -degeneracy means that the constraint thus obtained on will still depend sensitively on exactly what we choose to be the upper limit of that prior.
This exercise also highlights the danger of analytic marginalisation , a technique sometimes used on nuisance parameters in CosmoMC to shorten the computation time. Here, analytic integration of the posterior in the direction of a nuisance parameter is made possible by taking the lower and upper limits of the parameter’s top-hat prior to and respectively. Using this technique on the marginalisation of , we find a unimodal 1D posterior for whose 95% MCI of favours unambiguously the high region. Thus, analytic marginalisation can be very useful if the likelihood function itself sufficiently constrains the nuisance parameters. Otherwise, as we have seen here, the end results are potentially misleading.
Finally, we note that the model does not suffer these problems. Figure 8 shows the 2D marginal 68% and 95% MCIs for , , and , and the corresponding 1D marginal posteriors for case (iii). Here, although the correction parameter is slightly degenerate with the axion mass , it is independently well constrained by data. Importantly, even if data fails to constrain , we have a simple and well defined way to choose our prior on . Thus we conclude that the model is at present superior to the model for nonlinear correction in non-vanilla cosmologies.
In this paper we have explored two nonlinear correction and scale-dependent bias models—the model of reference  and the halo model-inspired model—in some detail. We have confronted them with a range of galaxy clustering data and cosmologies to determine the strengths and weaknesses of the models.
In the context of standard CDM cosmology, we find that both models perform equally well on present galaxy power spectrum data, in the sense that their corrective effects on the matter power spectrum are essentially identical. The case for nonlinear correction is very strong for the SDSS-4 LRG power spectrum. An indicative figure of merit is the minimum : fitting data up to , we find that changes from for 18 degrees of freedom without correction to for 17 degrees of freedom with correction, irrespective of the nonlinear model used. For 2dF and SDSS-2 main, however, the need for correction is marginal and subsists primarily because their respective estimates show better agreement with than without nonlinear correction. The preferred values of from SDSS-4 LRG, SDSS-2 main, and 2dF after correction, as well as from WMAP-3 can all be reconciled at 95% confidence, contrary to the case without correction.
Similar results are obtained for CDM cosmologies extended with a subdominant component of massive neutrino hot dark matter. Data again show no strong preference for either nonlinear correction model, nor do we find any detrimental degeneracy between the neutrino fraction and either nonlinear correction parameter. Cosmological neutrino mass determination is at the time being unaffected by our choice of nonlinear correction model.
However, if the subdominant free-streaming dark matter is in the form of relic thermal axions, a nontrivial degeneracy between the axion mass and the correction parameter renders the model highly pathological, so that our inference of depends sensitively on the prior we impose on . In contrast, the model, whose functional form is based on well motivated physics, does not suffer from this problem, and is arguably superior to the model. Note that we have used relic thermal axions here as an example. But our results may also be relevant for other light thermal relics whose temperature and hence abundance depend on the mass of the particle.
More precise data from future galaxy redshift surveys will eventually render these simplistic models inadequate to describe nonlinear evolution and scale-dependent biasing. For example, the damping of baryon acoustic oscillations due to nonlinear mode-coupling will need to be factored into the game at some stage [28, 43, 44]. The advent of wide- and deep-field weak gravitational lensing surveys in the next decade as an alternative probe of the large scale structure distribution will circumvent some of these nonlinearity issues. But galaxy redshift surveys will remain an important tool for the observation of baryon acoustic oscillations, and nonlinear evolution/scale-dependent bias modelling will continue to constitute an important aspect of the cosmological analysis machinery.
We thank Alexia Schulz and Robert E. Smith for useful comments on the manuscript. We acknowledge use of computing resources from the Danish Center for Scientific Computing (DCSC).
- Tegmark et al.  used , although strictly speaking is the more appropriate value for the real space power spectrum of SDSS-4 LRG. However, at the present level of precision, our tests show that adopting the correct only causes a statistically insignificant upward shift in the best-fit (), while the estimates of other cosmological parameters remain unaffected. Henceforth we shall use exclusively for both real and redshift space power spectra.
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