Issue 
A&A
Volume 631, November 2019



Article Number  L13  
Number of page(s)  6  
Section  Letters to the Editor  
DOI  https://doi.org/10.1051/00046361/201936373  
Published online  20 November 2019 
Letter to the Editor
Evidence for anisotropy of cosmic acceleration^{⋆}
^{1}
CNRS, UPMC, Institut d’Astrophysique de Paris, 98 bis Bld Arago, Paris, France
^{2}
Niels Bohr Institute, University of Copenhagen, Blegdamsvej 17, 2100 Copenhagen, Denmark
^{3}
Rudolf Peierls Centre for Theoretical Physics, University of Oxford, Parks Road, Oxford OX1 3PU, UK
email: s.sarkar@physics.ox.ac.uk
Received:
22
July
2019
Accepted:
18
October
2019
Observations reveal a “bulk flow” in the local Universe which is faster and extends to much larger scales than are expected around a typical observer in the standard ΛCDM cosmology. This is expected to result in a scaledependent dipolar modulation of the acceleration of the expansion rate inferred from observations of objects within the bulk flow. From a maximumlikelihood analysis of the Joint Lightcurve Analysis catalogue of Type Ia supernovae, we find that the deceleration parameter, in addition to a small monopole, indeed has a much bigger dipole component aligned with the cosmic microwave background dipole, which falls exponentially with redshift z: q_{0} = q_{m} + q_{d}.n̂ exp(z/S). The best fit to data yields q_{d} = −8.03 and S = 0.0262 (⇒d ∼ 100 Mpc), rejecting isotropy (q_{d} = 0) with 3.9σ statistical significance, while q_{m} = −0.157 and consistent with no acceleration (q_{m} = 0) at 1.4σ. Thus the cosmic acceleration deduced from supernovae may be an artefact of our being nonCopernican observers, rather than evidence for a dominant component of “dark energy” in the Universe.
Key words: cosmology: observations / dark energy / largescale structure of Universe
The code used here is available at: https://github.com/rameez3333/Dipole_JLA
© ESO 2019
1. Introduction
The foundations of the current standard model of cosmology date back nearly a century to when essentially no data were available. In particular the Universe was assumed to be exactly isotropic and homogeneous, with spacetime described by the maximally symmetric Friedmann–Lemaître–Robertson–Walker metric, and occupied by ideal fluids with purely diagonal energymomentum tensors (Peebles 1994). Subsequently it has been recognised that the distribution of galaxies, which is a biased tracer of the underlying distribution of the dominant dark matter, is rather inhomogeneous. Countsinspheres of galaxy catalogues have suggested that there is a transition to (statistical) homogeneity on scales exceeding ∼100 Mpc (Hogg et al. 2005; Scrimgeour et al. 2012), although sufficiently large volumes have not yet been surveyed to establish this definitively. This is however the expectation in the current standard cosmological model if the observed largescale structure has grown under gravity in the sea of dark matter, starting with an initially Gaussian random field of small density perturbations with an approximately scaleinvariant spectrum. Detailed observations of the temperature fluctuations in the cosmic microwave background (CMB) have broadly confirmed this model (Planck Collaboration I 2019). However several anomalies have been noted such as the lack of correlations on large angular scales, the quadrupoleoctupole alignment, and the hemispherical power asymmetry, which seem to imply a violation of statistical isotropy and scaleinvariance of primordial perturbations; nevertheless there is no consensus yet on either their physical nature or their origin (Schwarz et al. 2016).
In our real Universe there are “peculiar motions” due to the local inhomogeneity and anisotropy of surrounding structure. These are nonnegligible, for example our Local Group of galaxies moves with respect to the universal expansion at 620 ± 15 ∼ km s^{−1} towards ℓ = 271.9 ± 2° ,b = 29.6 ± 1.4°, as is inferred from the observed dipolar modulation of the CMB temperature (Kogut et al. 1993, Planck Collaboration I 2019). Moreover diverse observations reaching out as far as ∼300 Mpc, for example, by Lauer & Postman (1994), Hudson et al. (2004), Watkins et al. (2009), Lavaux et al. (2010), Feldman et al. (2010), Colin et al. (2011), Feindt et al. (2013), and Magoulas et al. (2016), have not seen the expected ∼1/r falloff of the peculiar velocity in the standard Λcold dark matter (CDM) cosmology. The odds of this happening by chance in that framework can be estimated by querying Hubble volume simulations of largescale structure formation, for example, Dark Sky (Skillman et al. 2014). Less than 1% of Milky Waylike observers should observe the bulk flow (> 250 km s^{−1} extending to z > 0.03) that we observe (Rameez et al. 2018). Thus we are not comoving observers but are “tilted” relative to the idealised Hubble flow (Tsagas 2010). The implications of this have been discussed for measurements of the Hubble parameter H_{0} (Hess & Kitaura 2014), but not for the inference of cosmic acceleration.
Since cosmological observables are formulated in the “CMB frame” in which the Universe is supposedly perfectly isotropic, it is in any case always necessary to correct what we measure from our relative moving frame. For example the observed redshifts of the Type Ia supernovae (SNe Ia) in catalogues like Joint Lightcurve Analysis (JLA; Betoule et al. 2014) have been corrected to convert from the heliocentric frame to the CMB frame. The methodology used follows earlier work (Conley et al. 2011) which used bulk flow observations made back in 2004 (Hudson et al. 2004) and moreover assumed that there is convergence to the CMB frame beyond 150 Mpc. Since this is not in accordance with subsequent deeper observations, we use only the heliocentric redshifts and reverse the corrections applied to the magnitudes to examine whether the deceleration parameter measured in our (bulk flow) rest frame can indeed differ from that of comoving observers in the model universe (Tsagas 2010). Such theoretical considerations imply (Tsagas 2011; Tsagas & Kadiltzoglou 2015) that there should be a dipole asymmetry in the derived cosmic deceleration parameter q_{0} towards the bulk flow direction. In this work we find a significant (3.9σ) indication of such a dipole, and also that the monopole in q_{0} decreases simultaneously in significance (to 1.4σ). Hence not only is the indication for acceleration statistically marginal (Nielsen et al. 2016), it probably arises because we are tilted observers located in a bulk flow, rather than due to the effect of a cosmological constant or dark energy.
2. Joint Lightcurve Analysis
We used the most uptodate publicly available sample of supernova lightcurve properties and directions: the SDSSII/SNLS3 JLA catalogue (Betoule et al. 2014). This consists of 740 spectroscopically confirmed SNe Ia, including several low redshift (z < 0.1) samples, three seasons of SDSSII (0.05 < z < 0.4), and three years of SNLS (0.2 < z < 1) data; these samples are all calibrated consistently in the Spectral Adaptive Lightcurve Template 2 (SALT2) scheme. This assigns three parameters to each supernova: the apparent magnitude ${m}_{B}^{*}$ at maximum in the restframe B band and the lightcurve shape and colour corrections, x_{1} and c. The distance modulus is then given by
$$\begin{array}{c}\hfill {\mu}_{\mathrm{SN}}={m}_{B}^{\ast}M+\alpha {x}_{1}\beta c,\end{array}$$(1)
where α and β are assumed to be constants, as is M the absolute SNe Ia magnitude, as befits a standard candle. In the standard ΛCDM cosmological model this is related to the luminosity distance d_{L} as
$$\begin{array}{cc}\hfill \mu & \equiv 25+5{log}_{10}({d}_{\mathrm{L}}/\mathrm{Mpc}),\phantom{\rule{1em}{0ex}}\mathrm{where},\hfill \\ \hfill {d}_{\mathrm{L}}& =(1+z)\frac{{d}_{\mathrm{H}}}{\sqrt{{\mathrm{\Omega}}_{k}}}\mathrm{sin}\left(\sqrt{{\mathrm{\Omega}}_{k}}{{\displaystyle \int}}_{0}^{z}\frac{{H}_{0}\mathrm{d}z\prime}{H(z\prime )}\right),\phantom{\rule{0.166667em}{0ex}}\mathrm{for}\phantom{\rule{0.166667em}{0ex}}{\mathrm{\Omega}}_{k}>0\hfill \\ \hfill & =(1+z){d}_{\mathrm{H}}{{\displaystyle \int}}_{0}^{z}\frac{{H}_{0}\mathrm{d}z\prime}{H(z\prime )},\phantom{\rule{0.166667em}{0ex}}\mathrm{for}\phantom{\rule{0.166667em}{0ex}}{\mathrm{\Omega}}_{k}=0\hfill \\ \hfill & =(1+z)\frac{{d}_{\mathrm{H}}}{\sqrt{{\mathrm{\Omega}}_{k}}}\mathrm{sinh}\left(\sqrt{{\mathrm{\Omega}}_{k}}{{\displaystyle \int}}_{0}^{z}\frac{{H}_{0}\mathrm{d}z\prime}{H(z\prime )}\right),\phantom{\rule{0.166667em}{0ex}}\mathrm{for}\phantom{\rule{0.166667em}{0ex}}{\mathrm{\Omega}}_{k}<0\hfill \\ \hfill {d}_{\mathrm{H}}& =c/{H}_{0},\phantom{\rule{1em}{0ex}}{H}_{0}\equiv 100h\phantom{\rule{3.33333pt}{0ex}}\mathrm{km}\phantom{\rule{0.166667em}{0ex}}{\mathrm{s}}^{1}{\mathrm{Mpc}}^{1},\hfill \\ \hfill H& ={H}_{0}\sqrt{{\mathrm{\Omega}}_{\mathrm{M}}{(1+z)}^{3}+{\mathrm{\Omega}}_{k}{(1+z)}^{2}+{\mathrm{\Omega}}_{\mathrm{\Lambda}}}\phantom{\rule{0.166667em}{0ex}}.\hfill \end{array}$$(2)
In this equation, d_{H} is the Hubble distance and H the Hubble parameter (H_{0} being its present value), and Ω_{M}, Ω_{Λ}, Ω_{k} are the matter, cosmological constant, and curvature densities in units of critical density. In the ΛCDM model these are related by the cosmic sum rule 1 = Ω_{M} + Ω_{Λ} + Ω_{k}. However we make no such model assumptions and simply expand the luminosity distance d_{L} in a Taylor series to examine its second derivative, i.e. the acceleration (see Sect. 3). This is because acceleration is a kinematic quantity and can be measured without making any assumptions about the dynamics underlying the universal expansion. There may be concern that such a Taylor expansion fails at high redshift, however we verified that d_{L} in the bestfit ΛCDM model differs by only 7% even at z = 1.3 (the highest redshift in the JLA sample), which is much less than the measurement uncertainty. Indeed the Taylor expansion fits the data just as well as ΛCDM.
Figure 1 is a Mollewide projection of the directions of the 740 SNe Ia in galactic coordinates. As a consequence of the diverse survey strategies of the subsamples that make up the JLA catalogue, its sky coverage is patchy and anisotropic. While the low redshift objects are spread out unevenly across the sky, the intermediate redshift objects from SDSS are mainly confined to a narrow disc at low declination, while the high redshift objects from SNLS are clustered along four specific directions.
Fig. 1. Sky distribution of the 4 subsamples of the JLA catalogue in galactic coordinates: SDSS (red dots), SNLS (blue dots), low redshift (green dots), and HST (black dots). The 4 big blue dots show clusters of many individual SNe Ia. The directions of the CMB dipole (star), the SMAC bulk flow (triangle) and the 2M++ bulk flow (inverted triangle) are also shown. 
The JLA analysis (Betoule et al. 2014) corrects the observed redshifts in the heliocentric frame, z_{hel}, in order to obtain the cosmological redshifts, z_{CMB}, after accounting for peculiar motions in the local Universe. These corrections are carried over unchanged from an earlier analysis (Conley et al. 2011), which in turn cites an earlier method (Neill et al. 2007) and the peculiar velocity model of Hudson et al. (2004). It is stated that the inclusion of these corrections allow SNe Ia with redshifts down to 0.01 to be included in the cosmological analysis, in contrast to earlier analyses (Riess et al. 2007) which employed only SNe Ia down to z = 0.023.
In Fig. 2 we scrutinise these corrections by exhibiting the velocity parameter 𝒞, defined as
$$\begin{array}{c}\hfill \mathcal{C}=[(1+{z}_{\mathrm{hel}})(1+{z}_{\mathrm{CMB}})(1+{z}_{\mathrm{d}})]\times c,\end{array}$$(3)
Fig. 2. Peculiar velocity corrections applied to the JLA catalogue. The velocity parameter 𝒞 in Eq. (3) is shown vs. the observed redshift. 
Fig. 3. Monopole and dipole components of the cosmological deceleration parameter (inferred from the JLA catalogue of 740 SNe Ia). The 1, 2, and 3σ contours (corresponding to −2 log ℒ/ℒ_{max} = 2.3, 6.18, and 11.8, respectively) are shown, profiling over all other parameters. The vertical scale for the magnitude of the dipole is compressed by ×10 relative to the horizontal scale for the monopole. The value of q_{0} for the standard ΛCDM model is shown as a blue star. 
where z_{hel} and z_{CMB} are as tabulated by JLA, while z_{d} is given by (Davis et al. 2011)
$$\begin{array}{c}\hfill {z}_{\mathrm{d}}=\sqrt{\frac{1{\mathit{v}}_{\mathrm{CMB}\odot}.\widehat{n}/c}{1+{\mathit{v}}_{\mathrm{CMB}\odot}.\widehat{n}/c}}1,\end{array}$$(4)
where v_{CMB − ⊙} is 369 km s^{−1} in the direction of the CMB dipole (Kogut et al. 1993) and $\widehat{n}$ is the unit vector in the direction of the supernova. It can be seen in Fig. 2 that SNe Ia beyond z ∼ 0.06 have been assumed to be stationary w.r.t. the CMB rest frame, and corrections applied only to those at lower redshifts. It is not clear how these corrections were made beyond z ∼ 0.04, which is the maximum extent to which the Streaming Motions of Abell Clusters (SMAC) sample (Hudson et al. 2004) extends. This has a bulk velocity of 687 ± 203 km s^{−1} towards ℓ = 260 ± 13° ,b = 0 ± 11° out to z = 0.04 at 90%C.L., and a bulk velocity of 372 ± 127 km s^{−1} towards ℓ = 273° ,b = 6° generated by sources beyond 200 h^{−1} Mpc (⇒z ≃ 0.064) at 98% C.L. If the peculiar velocity field is not discontinuous, the SNe Ia immediately outside this volume should have comparable velocities. Figure 2 indicates however that the JLA peculiar velocity corrections have arbitrarily assumed that the bulk flow abruptly disappears at this point. The JLA analysis (Betoule et al. 2014) allows SNe Ia beyond this distance to only have an uncorrelated velocity dispersion of cσ_{z} = 150 km s^{−1}. In the absence of any evidence of convergence to the CMB rest frame, this assumption is unjustified since it is very possible that the observed bulk flow stretches out to much larger scales. There have been persistent claims of a “dark flow” extending out to several hundreds of megaparsec (Kashlinsky et al. 2009, 2010, 2011), although this is still under debate. At any rate the value of cσ_{z} should be determined by fitting to the data, rather than put in by hand.
At this point it is worth noting the anisotropy of the JLA catalogue. Out of the 740 SNe Ia, 551 are in the hemisphere pointing away from the CMB dipole. With respect to the 372 ± 127 km s^{−1} bulk flow of the model (Hudson et al. 2004) from which the redshifts of the local SNe Ia have been corrected, only 108 are in the upper hemisphere while 632 are in the lower hemisphere. With respect to the direction of the abnormally high flow reported by 6dFGSv, the largest and most homogeneous peculiar velocity sample of nearly 9000 galaxies (Magoulas et al. 2016), 103 SNe Ia are in the upper hemisphere while 637 are in the lower hemisphere.
The subsequent Pantheon catalogue (Scolnic et al. 2018), which incorporates 308 additional SNe Ia (many from the PanSTARRS survey), continues to suffer from these problems. While the flow model (Carrick et al. 2015) from which the redshifts of the Pantheon sample have been corrected go out to z ∼ 0.067, this model has a residual bulk flow of 159 ± 23 km s^{−1} attributed to sources beyond z = 0.067, and 890 of the 1048 Pantheon SNe are in the hemisphere opposite to the direction of this flow.
Both JLA and Pantheon include SNe to which anomalously large peculiar velocity corrections have been applied at redshifts far higher than the limit to which the corresponding flow models extend. Two of the many such examples are SDSS2308 in JLA at z = 0.14 (the outlier in Fig. 2) and SN2246 in Pantheon at z = 0.194.
We used the heliocentric redshifts tabulated by JLA (Betoule et al. 2014) and subtracted out the bias corrections applied to ${m}_{B}^{*}$. For the Pantheon catalogue (Scolnic et al. 2018) the z_{hel} values and individual contributions to the covariance are not public, and moreover there are unresolved concerns about the accuracy of the data therein (Rameez 2019) so we cannot use it.
3. Cosmological analysis
We now compare the distance modulus (Eq. (1)) obtained from the JLA sample with the apparent magnitude (Eq. (2)) using the maximum likelihood estimator (MLE; Nielsen et al. 2016). Since we wish to analyse the data without making assumptions about the matter content or the dynamics, we use the kinematic Taylor series expansion of the luminosity distance up to the third term (Visser 2004) as follows:
$$\begin{array}{c}\hfill {d}_{\mathrm{L}}({z}_{\mathrm{hel}})=\frac{c{z}_{\mathrm{hel}}}{{H}_{0}}\{1+\frac{1}{2}[1{q}_{0}]{z}_{\mathrm{hel}}\frac{1}{6}[1{q}_{0}3{q}_{0}^{2}+{j}_{0}+\frac{k{c}^{2}}{{H}_{0}^{2}{a}_{0}^{2}}]{z}_{\mathrm{hel}}^{2}\},\end{array}$$(5)
where $q\equiv \ddot{a}a/{\dot{a}}^{2}$ is the cosmic deceleration parameter in the CMB frame, defined in terms of the scale factor of the universe a and its derivatives w.r.t. proper time, $j=\dot{\ddot{a}}/a{H}^{3}$ is the cosmic “jerk”, and $k{c}^{2}/({H}_{0}^{2}{a}_{0}^{2})$ is just Ω_{k}. We note that the last two appear together in the coefficient of the z^{3} term so these cannot be determined separately. In the ΛCDM model, q_{0} ≡ Ω_{M}/2 − Ω_{Λ}.
To look for a dipole in the deceleration parameter, we allow it to have a direction dependence written as
$$\begin{array}{c}\hfill q={q}_{\mathrm{m}}+{\mathit{q}}_{\mathrm{d}}.\widehat{n}\mathcal{F}(z,S),\end{array}$$(6)
where q_{m} and q_{d} are the monopole and dipole components, while $\widehat{n}$ is the direction of the dipole and ℱ(z, S) describes its scale dependence. We consider four representative functional forms as follows:

(a)
Constant: ℱ(z, S) = 1 independent of z,

(b)
Top hat: ℱ(z, S) = 1 for z < S, and 0 otherwise,

(c)
Linear: ℱ(z, S) = 1 − z/S, and

(d)
Exponential: ℱ(z, S) = exp(−z/S).
Owing to the anisotropic sky coverage of the dataset, it would be hard to find $\widehat{n}$ from the data, so we choose it to be along the CMB dipole direction. This is reasonable as the directions of the reported bulk flows (Hudson et al. 2004; Watkins et al. 2009; Lavaux et al. 2010; Feldman et al. 2010; Colin et al. 2011; Feindt et al. 2013; Magoulas et al. 2016) are all within ∼40° of each other and of the CMB dipole. Later we allow the direction to vary to demonstrate that our result is indeed robust.
We maximise a likelihood constructed earlier (March et al. 2011; Nielsen et al. 2016), simultaneously with respect to the four cosmological parameters q_{m}, j_{0} − Ω_{k}, q_{d}, and S, as well as the eight parameters that go into the standardisation of the SNe Ia candles: α, β, M_{0}, σ_{M0}, x_{1, 0}, σ_{x1, 0}, c_{0}, and σ_{c0}. While our analysis is frequentist, it is equivalent to the Bayesian hierarchical model of March et al. (2011), which indeed yielded the same result (Shariff et al. 2016) as the frequentist analysis of Nielsen et al. (2016) when applied to the JLA catalogue.
In Table 1 we show how this compares with using the prevalent constrained χ^{2} method used by, for example Betoule et al. (2014), wherein an arbitrary error σ_{int} is added to each data point and varied until a good fit (with χ^{2} = 1/d.o.f.) is obtained to the assumed model. This may be appropriate for parameter estimation, but not for model selection.
Tilted local universe, with σ_{z} set to zero, fitted to data with the constrained χ^{2} method.
However as seen in Table 2 the quality of fit improves further (−2 log ℒ_{max} decreases) when q_{0} is allowed to have a dipole. In the best fit where this has an exponentially decaying form ∝e^{−z/S}, the dipole q_{d} = −8.03 is much larger than the monopole q_{m} = −0.157 and its scale parameter is S = 0.0262, indicating that the impact of the bulk flow dominates over any isotropic acceleration out to z ∼ 0.1. Since Δ_{BIC} between the model with q_{d} = 0 and the model with q_{m} = 0 is 9.86, this constitutes strong evidence against a universe that is accelerating isotropically. In the presence of this dipole, q_{m} = 0 is disfavoured at only 1.4σ. In other words, in a universe in which we have theoretical reasons to expect a dipolar modulation in the deceleration parameter in the direction of our motion through the CMB, there is no significant evidence for a nonzero value of its monopole component. Figure 4 shows the 1, 2, and 3σ contours in the likelihood around the maximum as a function of q_{d} and q_{m}, profiling over all other parameters.
Tilted local universe, with σ_{z} set to zero, fitted to data with the MLE.
Fig. 4. Results of an a posteriori grid scan (left panel) varying the direction of the scaledependent dipolar modulation of the form ${q}_{0}={q}_{\mathrm{m}}+{\mathit{q}}_{\mathrm{d}}.\widehat{n}exp(z/S)$ in galactic coordinates. The bestfit direction is within 23° of the CMB dipole (indicated by a star) and −2 log ℒ (right panel) changes by just 3.22 between these two directions. 
We also study the effect of allowing an additional uncorrelated velocity dispersion cσ_{z} in the fit, rather than fixing it to be 150 km s^{−1} as in the JLA analysis (Betoule et al. 2014). As shown in Table 3 this improves the overall fit even further for cσ_{z} = 241 km s^{−1}; the bestfit dipole drops a little to q_{d} = −6.33, while the monopole is nearly unchanged at q_{m} = −0.154. The Δ_{BIC} between the model with q_{d} = 0 and that with q_{m} = 0 is 4.91, providing positive evidence against a universe that is accelerating isotropically. Our main result is thus robust in that the maximum likelihood estimator prefers to interpret the data as evidence of a dipole in the deceleration parameter aligned with the CMB dipole, rather than as an isotropic acceleration of the universe, which may indicate the presence of a cosmological constant.
Tilted local universe, with σ_{z} left floating, fitted to data with the MLE.
As an a posteriori test, we examine the direction dependence of this scaledependent dipolar modulation in q_{0}, by scanning the direction of q_{d} on a grid corresponding to a HEALpix (Gorski et al. 2005) map of nside=8. The bestfit direction is 23 degrees away from the CMB dipole, where q_{d} increases to −9.851 but −2 log ℒ improves by only 3.22. This demonstrates that the direction of the anisotropy we find is also robust.
4. Discussion
It has been observed (Bernal et al. 2017) that the deceleration parameter inferred from previous SNe Ia datasets has a redshift, and indeed directional dependence. This was interpreted as indicative of local anisotropy in the matter distribution, i.e. our being located in an asymmetric void. The refinement in the present work is that we consider a recent comprehensive database of SNe Ia and take into account all systematic effects as encoded in the covariance matrices provided (Betoule et al. 2014). Moreover we focus on the local velocity rather than the density field as this fully reflects the gravitational dynamics due to inhomogeneities. We can then explore the expected consequences of our being tilted, i.e. nonCopernican observers. Our analysis is guided by the suggestion that we may then infer acceleration even when the overall expansion rate is decelerating – a signature of which would be a dipolar modulation of the inferred q_{0} along the direction of the bulk flow.
The effect of peculiar velocities on SNe Ia cosmology has been discussed earlier (Hui & Greene 2006; Davis et al. 2011), however these studies relied on covariances that apply to Copernican observers. As we show elsewhere (Colin et al. 2019), the bulk flow we are embedded in is rare at a level of ≲1% (Rameez et al. 2018) according to the Dark Sky simulation (Skillman et al. 2014), but the conditional covariances can be up to a factor of ∼10 larger and introduce a preferred direction locally. This can make a much bigger impact on cosmological inferences than was found in previous studies. In particular the JLA analysis (Betoule et al. 2014) of the same dataset claimed that the effect of peculiar velocities is a tiny (< 0.1%) shift in the bestfit cosmological parameters.
In summary, the modelindependent evidence for acceleration of the Hubble expansion rate from the largest public catalogue of SNe Ia is only 1.4σ. This is in contrast to the claim (Scolnic et al. 2018) that acceleration is established by SNe Ia at > 6σ in the framework of the ΛCDM model. Moreover there is a significant (3.9σ) indication for a dipole in q_{0} towards the CMB dipole, which is indeed expected if the apparent acceleration is an artefact of our being located in a local bulk flow which extends out far enough to include most of the supernovae studied (Tsagas 2010, 2011; Tsagas & Kadiltzoglou 2015). Given the observational evidence that there is no convergence to the CMB frame as far out as redshift z ∼ 0.1, which includes half the known SNe Ia, this possibility must be taken seriously.
Acknowledgments
We thank the JLA collaboration for making all their data public and Dan Scolnic for correspondence concerning the Pantheon catalogue. We are grateful to Mike Hudson and Christos Tsagas for discussions. MR acknowledges a Carlsberg distinguished postdoctoral fellowship and hospitality at the Institut d’Astrophysique, Paris.
References
 Bernal, C., Cárdenas, V. H., & Motta, V. 2017, Phys. Lett. B, 765, 163 [NASA ADS] [CrossRef] [Google Scholar]
 Betoule, M., Kessler, R., Guy, J., et al. 2014, A&A, 568, A22 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Carrick, J., Turnbull, S. J., Lavaux, G., & Hudson, M. J. 2015, MNRAS, 450, 317 [NASA ADS] [CrossRef] [Google Scholar]
 Colin, J., Mohayaee, R., Sarkar, S., & Shafieloo, A. 2011, MNRAS, 414, 264 [NASA ADS] [CrossRef] [Google Scholar]
 Colin, J., Mohayaee, R., Rameez, M., & Sarkar, S. 2019, MNRAS, submitted [Google Scholar]
 Conley, A., Guy, J., Sullivan, M., et al. 2011, ApJS, 192, 1 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Davis, T. M., Hui, L., Frieman, J. A., et al. 2011, ApJ, 741, 67 [NASA ADS] [CrossRef] [Google Scholar]
 Feindt, U., Kerschhaggl, M., Kowalski, M., et al. 2013, A&A, 560, A90 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Feldman, H. A., Watkins, R., & Hudson, M. J. 2010, MNRAS, 407, 2328 [NASA ADS] [CrossRef] [Google Scholar]
 Gorski, K., Hivon, E., Banday, A., et al. 2005, ApJ, 622, 759 [NASA ADS] [CrossRef] [Google Scholar]
 Hellwing, W. A., Nusser, A., Feix, M., & Bilicki, M. 2017, MNRAS, 467, 2787 [NASA ADS] [Google Scholar]
 Hess, S., & Kitaura, F. S. 2014, MNRAS, 456, 4247 [NASA ADS] [CrossRef] [Google Scholar]
 Hogg, D. W., Eisenstein, D. J., Blanton, M. R., et al. 2005, ApJ, 624, 54 [NASA ADS] [CrossRef] [Google Scholar]
 Hudson, M. J., Smith, R. J., Lucey, J. R., & Branchini, E. 2004, MNRAS, 352, 61 [Google Scholar]
 Hui, L., & Greene, P. B. 2006, Phys. Rev. D, 73, 123526 [NASA ADS] [CrossRef] [Google Scholar]
 Kashlinsky, A., AtrioBarandela, F., Kocevski, D., & Ebeling, H. 2009, ApJ, 686, L49 [Google Scholar]
 Kashlinsky, A., AtrioBarandela, F., Ebeling, H., Edge, A., & Kocevski, D. 2010, ApJ, 712, L81 [NASA ADS] [CrossRef] [Google Scholar]
 Kashlinsky, A., AtrioBarandela, F., & Ebeling, H. 2011, ApJ, 732, 1 [NASA ADS] [CrossRef] [Google Scholar]
 Kogut, A., Lineweaver, C., Smoot, G. F., et al. 1993, ApJ, 419, 1 [NASA ADS] [CrossRef] [Google Scholar]
 Lauer, T. R., & Postman, M. 1994, ApJ, 425, 418 [NASA ADS] [CrossRef] [Google Scholar]
 Lavaux, G., Tully, R. B., Mohayaee, R., & Colombi, S. 2010, ApJ, 709, 483 [NASA ADS] [CrossRef] [Google Scholar]
 Magoulas, C., Springob, C., Colless, M., et al. 2016, Proc. IAU Symp., 308, 336 [NASA ADS] [Google Scholar]
 March, M., Trotta, R., Berkes, P., Starkman, G., & Vaudrevange, P. 2011, MNRAS, 418, 2308 [NASA ADS] [CrossRef] [Google Scholar]
 Neill, J. D., Hudson, M. J., & Conley, A. 2007, ApJ, 661, L123 [NASA ADS] [CrossRef] [Google Scholar]
 Nielsen, J. T., Guffanti, A., & Sarkar, S. 2016, Sci. Rep., 6, 35596 [NASA ADS] [CrossRef] [PubMed] [Google Scholar]
 Peebles, P. J. E. 1994, Principles of Physical Cosmology (Princeton University Press) [Google Scholar]
 Perlmutter, S., Aldering, G., Goldhaber, G., et al. 1999, ApJ, 517, 565 [NASA ADS] [CrossRef] [Google Scholar]
 Planck Collaboration I. 2019, A&A, in press, https://doi.org/10.1051/00046361/201833880 [Google Scholar]
 Rameez, M. 2019, ArXiv eprints [arXiv:1905.00221] [Google Scholar]
 Rameez, M., Mohayaee, R., Sarkar, S., & Colin, J. 2018, MNRAS, 477, 1772 [NASA ADS] [CrossRef] [Google Scholar]
 Riess, A. G., Filippenko, A. V., Challis, P., et al. 1998, AJ, 116, 1009 [NASA ADS] [CrossRef] [Google Scholar]
 Riess, A. G., Strolger, L. G., Casertano, S., et al. 2007, ApJ, 659, 98 [NASA ADS] [CrossRef] [Google Scholar]
 Rubin, D., & Hayden, B. 2016, ApJ, 833, L30 [NASA ADS] [CrossRef] [PubMed] [Google Scholar]
 Scolnic, D. M., Jones, D. O., Rest, A., et al. 2018, ApJ, 859, 101 [NASA ADS] [CrossRef] [Google Scholar]
 Scrimgeour, M. I., Davis, T., Blake, C., et al. 2012, MNRAS, 425, 116 [NASA ADS] [CrossRef] [Google Scholar]
 Shariff, H., Jiao, X., Trotta, R., & van Dyk, D. A. 2016, ApJ, 827, 1 [NASA ADS] [CrossRef] [Google Scholar]
 Skillman, S. W., Warren, M. S., & Turk, M. J. 2014, ArXiv eprints [arXiv:1407.2600] [Google Scholar]
 Schwarz, G. 1978, Ann. Stat., 6, 461 [Google Scholar]
 Schwarz, D. J., Copi, C. J., Huterer, D., & Starkman, G. D. 2016, Class. Quant. Grav., 33, 184001 [NASA ADS] [CrossRef] [Google Scholar]
 Tsagas, C. 2010, MNRAS, 405, 503 [NASA ADS] [Google Scholar]
 Tsagas, C. 2011, Phys. Rev. D, 84, 063503 [NASA ADS] [CrossRef] [Google Scholar]
 Tsagas, C., & Kadiltzoglou, M. I. 2015, Phys. Rev. D, 92, 043515 [NASA ADS] [CrossRef] [Google Scholar]
 Tutusaus, I., Lamine, B., Dupays, A., & Blanchard, A. 2017, A&A, 602, A73 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Visser, M. 2004, Class. Quant. Grav., 21, 2603 [NASA ADS] [CrossRef] [Google Scholar]
 Watkins, R., Feldman, H. A., & Hudson, M. J. 2009, MNRAS, 392, 743 [NASA ADS] [CrossRef] [Google Scholar]
 Watkins, R., & Feldman, H. A. 2015, MNRAS, 447, 132 [NASA ADS] [CrossRef] [Google Scholar]
Appendix A: Redshiftdependence of lightcurve fitting parameters
In this work we have used a statistical approach as well as the treatment of lightcurve parameters espoused by Nielsen et al. (2016). These authors were criticised by Rubin & Hayden (2016) for using redshiftindependent distributions for x_{1} and c. In this respect we note the following:
1. The JLA analysis determined the relationship between the luminosity distance and redshift for SNe Ia. To inspect a posteriori the distribution of two (x_{1} and c) out of the three ingredients that go into standardising SNe Ia and then add empirical terms in the fit to describe their sample dependence and redshift evolution, is fundamentally against the principles of blind hypothesis testing, especially since no such dependence had been suggested by Betoule et al. (2014).
2. Nevertheless we carry out the same 22parameter fit (Rubin & Hayden 2016) for comparison and present the results in Table A.1. While the log maximum likelihood ratio does improve for these fits, this parameterisation increases the significance of the dipole in q_{0} to 4.7σ (likelihood ratio of 18.3) and reduces further the significance of a monopole.
Fits to the JLA catalogue allowing for sample and redshiftdependence of SNe Ia parameters.
3. The addition of parameters to improve the quality of a fit and obtain a desired outcome have to be justified by physical and/or information theoretic arguments. The additional parameters of Rubin & Hayden (2016) can be justified by the Akaike information criterion but not by the stricter Bayesian information criterion. This also applies to the two additional parameters we introduce (q_{d} and S) but these are physically motivated for a tilted observer (Tsagas 2011; Tsagas & Kadiltzoglou 2015).
4. If the lightcurve parameters x_{1} and c are allowed to be sample or redshiftdependent we can ask why the absolute magnitude of SNe Ia should also not be sample or redshiftdependent. Allowing this of course undermines their use as standard candles and the data is then unsurprisingly consistent with no acceleration (Tutusaus et al. 2017), as seen in Table A.1.
Appendix B: Uncertainties
The JLA covariance matrix includes uncertainties from, for example the lightcurve template fitting process, calibration uncertainties, and dust extinction in the Galaxy, together with the expected dispersion resulting from peculiar velocities (which mainly affects low redshift SNe) and lensing (which mainly affects high redshift SNe Ia) and the propagated uncertainties from the flow model from which the SN by SN peculiar velocity corrections are performed. In addition it is also necessary to fit for a global intrinsic dispersion as in previous analyses (March et al. 2011). We use heliocentric redshifts in this analysis and thus do not include uncertainties related to the peculiar velocity corrections based on the flow model. The redshift dependence of the dispersions in the fit are shown in Fig. B.1.
Fig. B.1. Different sources of intrinsic dispersion in magnitude σ_{m} that enter cosmological fits of JLA data. On top of the global σ_{int}, SNe Ia are given a dispersion σ_{lens} proportional to redshift to account for lensing, while low redshift SNe Ia are selectively more dispersed by σ_{z} to account for peculiar velocity effects. 
All Tables
Tilted local universe, with σ_{z} set to zero, fitted to data with the constrained χ^{2} method.
Fits to the JLA catalogue allowing for sample and redshiftdependence of SNe Ia parameters.
All Figures
Fig. 1. Sky distribution of the 4 subsamples of the JLA catalogue in galactic coordinates: SDSS (red dots), SNLS (blue dots), low redshift (green dots), and HST (black dots). The 4 big blue dots show clusters of many individual SNe Ia. The directions of the CMB dipole (star), the SMAC bulk flow (triangle) and the 2M++ bulk flow (inverted triangle) are also shown. 

In the text 
Fig. 2. Peculiar velocity corrections applied to the JLA catalogue. The velocity parameter 𝒞 in Eq. (3) is shown vs. the observed redshift. 

In the text 
Fig. 3. Monopole and dipole components of the cosmological deceleration parameter (inferred from the JLA catalogue of 740 SNe Ia). The 1, 2, and 3σ contours (corresponding to −2 log ℒ/ℒ_{max} = 2.3, 6.18, and 11.8, respectively) are shown, profiling over all other parameters. The vertical scale for the magnitude of the dipole is compressed by ×10 relative to the horizontal scale for the monopole. The value of q_{0} for the standard ΛCDM model is shown as a blue star. 

In the text 
Fig. 4. Results of an a posteriori grid scan (left panel) varying the direction of the scaledependent dipolar modulation of the form ${q}_{0}={q}_{\mathrm{m}}+{\mathit{q}}_{\mathrm{d}}.\widehat{n}exp(z/S)$ in galactic coordinates. The bestfit direction is within 23° of the CMB dipole (indicated by a star) and −2 log ℒ (right panel) changes by just 3.22 between these two directions. 

In the text 
Fig. B.1. Different sources of intrinsic dispersion in magnitude σ_{m} that enter cosmological fits of JLA data. On top of the global σ_{int}, SNe Ia are given a dispersion σ_{lens} proportional to redshift to account for lensing, while low redshift SNe Ia are selectively more dispersed by σ_{z} to account for peculiar velocity effects. 

In the text 
Current usage metrics show cumulative count of Article Views (fulltext article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 4896 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.