Azimuthal Anisotropy Distributions in High-Energy Collisions

# Azimuthal Anisotropy Distributions in High-Energy Collisions

Li Yan    Jean-Yves Ollitrault CNRS, URA2306, IPhT, Institut de physique théorique de Saclay, F-91191 Gif-sur-Yvette, France    Arthur M. Poskanzer Lawrence Berkeley National Laboratory, Berkeley, California, 94720
July 19, 2019
###### Abstract

Elliptic flow in ultrarelativistic heavy-ion collisions results from the hydrodynamic response to the spatial anisotropy of the initial density profile. A long-standing problem in the interpretation of flow data is that uncertainties in the initial anisotropy are mingled with uncertainties in the response. We argue that the non-Gaussianity of flow fluctuations in small systems with large fluctuations can be used to disentangle the initial state from the response. We apply this method to recent measurements of anisotropic flow in Pb+Pb and p+Pb collisions at the LHC, assuming linear response to the initial anisotropy. The response coefficient is found to decrease as the system becomes smaller and is consistent with a low value of the ratio of viscosity over entropy of . Deviations from linear response are studied. While they significantly change the value of the response coefficient they do not change the rate of decrease with centrality. Thus, we argue that the estimate of is robust against non-linear effects.

## I Introduction

The large magnitude of elliptic flow, , in relativistic heavy-ion collisions at RHIC Ackermann:2000tr () and LHC Aamodt:2010pa () has long been recognized as a signature of hydrodynamic behavior of the strongly-interacting quark-gluon plasma Kolb:2003dz (). is understood as the hydrodynamic response to the initial anisotropy, , of the initial density profile Ollitrault:1992bk (). However, the magnitude of this anisotropy is poorly constrained theoretically Hirano:2005xf (); Lappi:2006xc (). This uncertainty hinders the extraction of the properties of the quark-gluon plasma from experimental data Luzum:2008cw (); Heinz:2013th ().

The statistical properties of anisotropic flow are now precisely known Jia:2014jca (). The ATLAS collaboration has analyzed the full probability distribution of , and in Pb+Pb collisions for several centrality windows Aad:2013xma (). In p+Pb collisions, information is less detailed, but the first moments of the distribution of have been measured Chatrchyan:2013nka (). Our goal is to make use of these measurements to separate the initial state from the response without assuming any particular model of the initial conditions – by only using a simple functional form which goes to zero at the geometric limits of and .

In theory, one can describe the particles emitted from a collision with an underlying probability distribution Luzum:2013yya (). Anisotropic flow, , is defined as the Fourier coefficient of the azimuthal probability distribution :

 Vn=vneinΨn≡12π∫2π0P(φ)einφdφ, (1)

where we have used a complex notation Ollitrault:2012cm (); Teaney:2013dta (). Note that the underlying probability distribution and fluctuate event to event, but they are both theoretical quantities which cannot be measured on an event-by-event basis. The particles that are detected in an event represent a finite sample of , and the measurement of the probability distribution of involves a nontrivial unfolding of statistical fluctuations Aad:2013xma ().

## Ii Distribution of εn

We assume that the fluctuations of for are due to fluctuations of the initial anisotropy in the corresponding harmonic, defined by Teaney:2010vd ()

 En=εneinΦn≡−∫rneinϕρ(r,ϕ)rdrdϕ∫rnρ(r,ϕ)rdrdϕ. (2)

where is the energy density near midrapidity shortly after the collision, and are polar coordinates in the transverse plane, in a coordinate system where the energy distribution is centered at the origin.

We assume for the moment that in a given event is determined by linear response to the initial anisotropy, , where is a response coefficient which does not fluctuate event to event. Event-by-event hydrodynamic calculations Niemi:2012aj () show that this is a very good approximation for . Within this approximation, it has already been shown that one can rule out particular models of the initial density using either a combined analysis Alver:2010dn (); Retinskaya:2013gca () of elliptic flow and triangular flow Alver:2010gr () data, or the relative magnitude of elliptic flow fluctuations Alver:2006wh (); Alver:2010rt (); Renk:2014jja (). Our goal is to show that one can extract both and the distribution of from data. We hope to show that this is true even if we relax the linear assumption. We make use of the recent observation that the distribution of is to a large extent universal Yan:2013laa (); Yan:2014afa () and can be characterized by two parameters.

Both the magnitude and direction of fluctuate event to event. The simplest parametrization of these fluctuations is a two-dimensional Gaussian probability distribution which, upon integration over azimuthal angle, yields the Bessel-Gaussian distribution Voloshin:2007pc ():

 p(εn)=εnσ2I0(ε0εnσ2)exp(−ε20+ε2n2σ2), (3)

where is the mean anisotropy in the reaction plane, which vanishes by symmetry for odd , and is the typical magnitude of eccentricity fluctuations around this mean anisotropy. Both and depend on the harmonic .

In a previous publication Yan:2014afa (), we have introduced an alternative parametrization, the Elliptic Power distribution:

 p(εn)=2αεnπ(1−ε20)α+12∫π0(1−ε2n)α−1dϕ(1−ε0εncosϕ)2α+1, (4)

where describes the fluctuations and is approximately proportional to the number of sources in an independent-source model Ollitrault:1992bk (). The parameter depends on . When and , Eq. (4) reduces to Eq. (3) with . Its support is the unit disk: it naturally takes into account the condition which follows from the definition, Eq. (2). For this reason, it is a better parametrization than the Bessel-Gaussian, in particular for large anisotropies. Eq. (4) has been shown to fit various initial-state models Yan:2014afa (). Note that is not strictly equal to the mean reaction plane eccentricity for the Elliptic Power distribution, but the difference is small for Pb+Pb collisions Yan:2014afa ().

When the anisotropy is solely due to fluctuations, , the Bessel-Gaussian reduces to a Gaussian distribution:

 p(εn)=εnσ2exp(−ε2n2σ2), (5)

and the Elliptic Power distribution reduces to the Power distribution Yan:2013laa ():

 p(εn)=2αεn(1−ε2n)α−1. (6)

## Iii Distribution of vn

The probability distribution of anisotropic flow, , is obtained from the distribution of the initial anisotropy by

 P(vn)=dεndvnp(εn). (7)

Assuming , this becomes:

 P(vn)=1κnp(vnκn). (8)

In this case the distribution is rescaled by the response coefficient . Figure 1 displays the probability distribution of and in various centrality windows Aad:2013xma () together with fits using rescaled Bessel-Gaussian and Elliptic Power distributions for , and rescaled Gaussian and Power distributions for . Both parametrizations give very good fits to and data for the most central bins shown on the figure.111The fits do not converge below () centrality for (), which reflects the fact that the distributions become very close to Bessel-Gaussian (Gaussian). As the centrality percentile increases, however, the quality of the Bessel-Gaussian fit becomes increasingly worse, which is reflected by the large of the fit, and also clearly seen in the tail of the distribution: it systematically overestimates the distribution for large anisotropies. On the other hand, the Elliptic Power fit is excellent for all centralities. In particular, it falls off more steeply for large , in close agreement with the data.

Note that the Bessel-Gaussian distribution Eq. (3) is scale invariant: rescaling it by amounts to multiplying both and by , so that the fit is degenerate: only the products and can be determined. Therefore the Bessel-Gaussian fit to ATLAS data is in practice a 2-parameter fit for , and a 1-parameter fit for . On the other hand, the Elliptic Power fit is not degenerate because of the non-Gaussian cut-off at , and returns both the response coefficient and the parameters pertaining to the shape, namely and (for ). However, the fit parameters are still correlated in the sense that the combinations and (for ) have much smaller errors than each individual parameter.

## Iv Experimental Errors

Our ability to separate the response from the initial eccentricity thus lies in the difference between the Bessel-Gaussian and the Elliptic Power fits, that is, in the non-Gaussianity of flow fluctuations. Since the difference is small, errors must be carefully evaluated.

The ATLAS collaboration reports the statistical error, the systematic error on the mean , and the systematic error on the relative standard deviation . The first systematic error is an error on the scale of the distribution, while the second is an error on its shape. The error on the scale directly translates into an error of the response coefficient , of the same relative magnitude. Since our analysis uses the deviations from a Gaussian shape, the dominant source of error is —by far— the error on the shape. In order to estimate the corresponding error on our fit parameters, we distort the distribution of in such a way that the mean is unchanged, and is increased or decreased by the experimental uncertainty. This is done in practice by shifting the values of the bins according to , where is a small non-linear shift. We choose the ansatz , where is the tail of the distribution, is chosen in such a way that is unchanged, and is chosen in such a way that is increased or decreased by the systematic error. This non-linear transformation leaves the minimum and maximum values of invariant.

## V Parameters of the Distributions

Figure 2 displays the value of the response coefficients and as a function of the centrality percentile. They are smaller than unity, with , in line with expectations from hydrodynamic calculations Niemi:2012aj (), and decrease as a function of the centrality percentile, which is the general behavior expected from viscous corrections to local equilibrium Voloshin:1999gs (); Drescher:2007cd (). We estimate that the low- cut of ATLAS at 0.5 GeV increases by a factor 1.4 to 1.5. The systematic error for is very large and therefore not shown: for most bins, the upper error bar goes all the way to infinity. Now, if one takes the limit while keeping the rms constant, in Eq. (6) also goes to infinity and the Power distribution reduces to a Gaussian distribution Eq. (5). Therefore the ATLAS distributions are compatible with Gaussians within systematic errors.

The other parameters of the fit to distributions, namely, and , characterize the shape of the distribution. They are displayed in Fig. 3 as a function of the collision centrality. increases smoothly with the centrality percentile: extrapolation to the most central collisions (where the fit does not converge) gives , as required by azimuthal symmetry.

Figure 3 also displays comparisons with the Glauber Miller:2007ri (); Broniowski:2007ft (); Alver:2008aq () and IP-Glasma Schenke:2012fw (); Schenke:2013aza () models. These models are shown as shaded bands. The bands correspond to the fact that the Elliptic Power distribution does not exactly fit the distribution of for that particular model. Specifically, the dashed line at the edge of the band is the value returned by a 2-parameter Elliptic Power fit to the distribution of . The full line at the other edge of the band is the value that the fit to the distribution would return if , with given by that model. If one assumes linear response, ATLAS data deviate from both models.

## Vi Cumulants

For p+Pb collisions, the full distribution of has not been measured, but only its first cumulants Borghini:2001vi (); Bilandzic:2010jr () and  Aad:2013fja (); Chatrchyan:2013nka (); Abelev:2014mda (). Assuming linear response to the initial eccentricity, each measured cumulant is proportional to the corresponding cumulant of the initial eccentricity Miller:2003kd (), , for … The eccentricity in p+Pb collisions is solely due to fluctuations Bozek:2011if (); Bozek:2012gr (), therefore Eqs. (5) and (6) apply. While cumulants of order 4 and higher vanish for the Gaussian distribution Eq. (5), the Power distribution Eq. (6) always gives  Yan:2013laa (). We again use this non-Gaussianity to disentangle the initial state from the response: We extract from the measured ratio  Yan:2013laa (). The rms anisotropy is then obtained as  Yan:2013laa (). One finally obtains for the Power distribution:

 κn=vn{2}εn{2}=vn{2} ⎷2(vn{2}vn{4})4−1. (9)

The values of extracted from CMS p+Pb data Chatrchyan:2013nka () using this equation are also displayed in Fig. 2. We multiply them by a factor to correct for the different low- cut ( GeV/) assuming a linear dependence of on . We plot p+Pb data at the equivalent centralities, determined according to the number of charged tracks Chatrchyan:2013nka (). General arguments have been put forward which suggest that the hydrodynamic response should be identical for p+Pb and Pb+Pb at the same equivalent centrality Basar:2013hea (). Once rescaled, the p+Pb slope is in line with Pb+Pb results, albeit somewhat steeper.

Note that the fit parameters can also be obtained from cumulants for in Pb+Pb collisions using Eq. (9). For , there is a third parameter , therefore one needs a third cumulant . and , which control the shape of the distribution and its non-Gaussian features, can be extracted from the ratios and using the Elliptic Power distribution (Eq. (A5) of Ref. Yan:2014afa ()). Note that while the Bessel-Gaussian Eq. (3) gives  Bzdak:2013rya (), the Elliptic Power distribution always gives . We have checked that and thus extracted from cumulant ratios are essentially identical to those obtained by fitting the distribution of . This approach has the advantage that cumulants can be analyzed without any unfolding procedure Bilandzic:2010jr () but may suffer from non-flow effects.

## Vii Deviations from linear scaling

We now discuss the effect of deviations from linear eccentricity scaling of anisotropic flow. Because of such deviations, the shape of the distribution is not exactly the same as that of the distribution, as already noted in event-by-event hydrodynamic calculations Schenke:2014zha (). There are two distinct types of non-linearities: can be a function of which is not exactly linear, or can depend on properties of the initial state other than . We study these effects in turn.

Adding a quadratic term would be equivalent to rotating the distribution 90 degrees or changing the sign of . Thus the first significant non-linear term is the cubic:

 v2=κ2ε2+κ′κ2ε32. (10)

Several hydrodynamic calculations show evidence that  Bhalerao:2005mm (); Alver:2010dn (); Paatelainen:2014 (), but no quantitative analysis has been done yet. One typically expects to depend mildly on centrality. When fitting the experimental distributions with the added parameter of the cubic term, had large errors but was in the range from 0 to 0.15. Thus we fixed at 0.10 and plotted the values also in Fig. 2. The effect of the non-linear response is to reduce the linear response coefficient , essentially by a constant factor. In the case where the distribution of is the Power distribution (6) and in the limit , the relative change of is

 Δκ2κ2=−2κ′ (11)

to leading order.222This result is obtained by inserting Eq. (10) into Eq. (9) and using the approximate relation for . With the Elliptic-Power distribution, the relative effect is also as can be seen in Fig. 2. Note that this non-linear correction to the response is much larger than one would naively expect from Eq. (10): the relative magnitude of the cubic term , yet it produces an effect of order . The reason is that the non-linear response contributes to the non-Gaussianity of flow fluctuations.

We now discuss deviations from linearity due to the fact that is not entirely determined by  Teaney:2010vd (). One can generally decompose the flow as , where is uncorrelated with the initial eccentricity . There can be various contributions to from non-linear coupling between different harmonics Teaney:2012ke () or radial modulations of the initial density Teaney:2010vd (). In order to estimate their effect on the hydrodynamic response, we further assume that is a Gaussian noise. Then, the distribution of is a rescaled Elliptic-Power distribution, convoluted with a Gaussian: the deviation from linearity here results in a Gaussian smearing of the distribution.

A quantitative measure of the magnitude of is the Pearson correlation coefficient between the anisotropic flow and the initial anisotropy, defined as

 rn ≡ ⟨VnE∗n⟩√⟨|Vn|2⟩⟨|En|2⟩ (12) = (1+⟨|Xn|2⟩κ2n⟨|En|2⟩)−1/2, (13)

where angular brackets denote an average value over events in a centrality class. Our analysis assumes the maximum correlation, . Event-by-event hydrodynamic calculations show that there are small deviations around eccentricity scaling Holopainen:2010gz ().

Ideal hydrodynamics Gardim:2011xv () gives for elliptic flow. However, the correlation between and has been shown to be significantly larger in viscous hydrodynamics Niemi:2012aj (), and a value seems reasonable, but there is to date no quantitative estimate of as defined in Eq. (12).

The effect on the fit parameters can be obtained using the fact that the rms flow is increased by the noise, while higher-order cumulants and (see below Sec. VI) are unchanged. We find that a decrease of by 1% results in an decrease of the extracted by 6% to 9%, depending on the centrality, the effect being maximum in the 20-30% centrality range. The value of found in ideal hydrodynamic calculations Gardim:2011xv () depends mildly on centrality and is closest to 1 also in the 20-30% centrality range. Therefore one can conjecture —this should eventually be confirmed by detailed calculations— that the effect of the noise is to reduce the extracted response essentially by a constant factor, independent of centrality.

Note that the cubic response in Eq. (10) does not contribute to to first order in , so that the two effects are in practice well separated.

The conclusion is that deviations from linear eccentricity scaling all make smaller, by a factor which can be significant, but depends little on centrality. This is of crucial importance for the extraction of the viscosity over entropy ratio (see below). The decrease in makes larger and smaller (see Fig. 3), thereby improving compatibility with existing initial-state models.

## Viii Viscous Hydro

We now compare our result for with hydrodynamic calculations. To the extent that anisotropic flow scales linearly with eccentricity, the value of the response coefficient is independent of initial conditions. In ideal hydrodynamics, scale invariance implies that is independent of the system size, i.e., independent of centrality. Deviations from thermal equilibrium generally result in a reduction of the flow which is stronger for peripheral collisions Voloshin:1999gs (); Drescher:2007cd (). In a hydrodynamic calculation Heinz:2013th (), such deviations are due to the shear viscosity Luzum:2008cw () and, to a lesser extent, to the freeze-out procedure at the end of the hydrodynamic expansion. Therefore the dependence of on centrality in Fig. 2 can be used to estimate the shear viscosity over entropy ratio of the quark-gluon plasma. We use the same hydrodynamic code as in Ref. Teaney:2012ke () to estimate . The resulting values are significantly smaller than the data in Fig. 2. Since we have shown that deviations from linear eccentricity scaling reduce without altering its centrality dependence, we compensate for this effect, and the low cut of the ATLAS data, by multiplying our hydrodynamic result by a constant, while tuning the viscosity so as to match the centrality dependence of . Since the systematic errors on are so large, we only fit . The smooth solid lines in Fig. 2 are obtained with . The dashed lines show the sensitivity to . This extracted value of is consistent with that reported in the literature Heinz:2013th (), using specific models of the initial state. For sake of illustration, we also show the result for with the same and the same overall normalization factor as for . We recall that systematic errors on from experimental data are very large so that no conclusion on can be drawn from these data alone.

## Ix Summary

We have shown that a rescaled Elliptic Power distribution fits the measured distributions of elliptic and triangular flows in Pb+Pb collisions at the LHC. These distributions become increasingly non-Gaussian as the anisotropy increases. We have used this non-Gaussianity to disentangle for the first time the initial anisotropy from the response without assuming any particular model of initial conditions – just using a simple functional form which meets the geometrical constrants of eccentricity.

This is another aspect of the analogy between heavy-ion physics and cosmology Mishra:2007tw (); Dusling:2011rz (), where initial quantum fluctuations give rise to correlations, and the non-Gaussian statistics of these correlations can be used to unravel the properties of the initial state Maldacena:2002vr (); Bartolo:2004if (); Ade:2013ydc (). The non-Gaussianity is stronger for smaller systems, which is an incentive to analyze flow in smaller collision systems.

We have found that the hydrodynamic response to ellipticity has the expected overall magnitude and centrality dependence: it decreases with centrality percentage. A somewhat similar slope is found for p+Pb collisions. This decrease can be attributed to the viscous suppression of . Comparison with hydrodynamic calculations supports a low value of the viscosity over entropy ratio, .

The present study can be improved by constraining the cubic response coefficient in Eq. (10) as well as the Pearson coefficient due to other non-linear terms in Eq. (12). This could be done in future hydrodynamic calculations. Taking into account these nonlinear terms will decrease the magnitude of the response and therefore improve the agreement with hydrodynamic calculations. However, we have argued that this decrease is essentially a constant factor, independent of centrality, so that our estimate of is likely to be robust. Our study is a first step toward the extraction of the viscosity over entropy ratio of the quark-gluon plasma from experimental data, without any prior knowledge of the initial state.

###### Acknowledgements.
We thank M. Luzum and S. Voloshin for extensive discussions and suggestions. In particular, we thank S. Voloshin for useful comments on the manuscript. JYO thanks the MIT LNS for hospitality. LY is funded by the European Research Council under the Advanced Investigator Grant ERC-AD-267258. AMP was supported by the Director, Office of Nuclear Science of the U.S. Department of Energy.

## References

• (1) K. H. Ackermann et al. [STAR Collaboration], Phys. Rev. Lett. 86, 402 (2001) [nucl-ex/0009011].
• (2) K. Aamodt et al. [ALICE Collaboration], Phys. Rev. Lett. 105, 252302 (2010) [arXiv:1011.3914 [nucl-ex]].
• (3) P. F. Kolb and U. W. Heinz, In *Hwa, R.C. (ed.) et al.: Quark gluon plasma* 634-714 [nucl-th/0305084].
• (4) J. Y. Ollitrault, Phys. Rev. D 46, 229 (1992).
• (5) T. Hirano, U. W. Heinz, D. Kharzeev, R. Lacey and Y. Nara, Phys. Lett. B 636, 299 (2006) [nucl-th/0511046].
• (6) T. Lappi and R. Venugopalan, Phys. Rev. C 74, 054905 (2006) [nucl-th/0609021].
• (7) M. Luzum and P. Romatschke, Phys. Rev. C 78, 034915 (2008) [Erratum-ibid. C 79, 039903 (2009)] [arXiv:0804.4015 [nucl-th]].
• (8) U. Heinz and R. Snellings, Ann. Rev. Nucl. Part. Sci. 63, 123 (2013) [arXiv:1301.2826 [nucl-th]].
• (9) J. Jia, arXiv:1407.6057 [nucl-ex].
• (10) G. Aad et al. [ATLAS Collaboration], JHEP 1311, 183 (2013) [arXiv:1305.2942 [hep-ex]].
• (11) S. Chatrchyan et al. [CMS Collaboration], Phys. Lett. B 724, 213 (2013) [arXiv:1305.0609 [nucl-ex]].
• (12) M. Luzum and H. Petersen, J. Phys. G 41, 063102 (2014) [arXiv:1312.5503 [nucl-th]].
• (13) J. Y. Ollitrault and F. G. Gardim, Nucl. Phys. A 904-905, 75c (2013) [arXiv:1210.8345 [nucl-th]].
• (14) D. Teaney and L. Yan, Phys. Rev. C 90, 024902 (2014) [arXiv:1312.3689 [nucl-th]].
• (15) D. Teaney and L. Yan, Phys. Rev. C 83, 064904 (2011) [arXiv:1010.1876 [nucl-th]].
• (16) H. Niemi, G. S. Denicol, H. Holopainen and P. Huovinen, Phys. Rev. C 87, 054901 (2013) [arXiv:1212.1008 [nucl-th]].
• (17) B. H. Alver, C. Gombeaud, M. Luzum and J. Y. Ollitrault, Phys. Rev. C 82, 034913 (2010) [arXiv:1007.5469 [nucl-th]].
• (18) E. Retinskaya, M. Luzum and J. Y. Ollitrault, Phys. Rev. C 89, 014902 (2014) [arXiv:1311.5339 [nucl-th]].
• (19) B. Alver and G. Roland, Phys. Rev. C 81, 054905 (2010) [Erratum-ibid. C 82, 039903 (2010)] [arXiv:1003.0194 [nucl-th]].
• (20) B. Alver et al. [PHOBOS Collaboration], Phys. Rev. Lett. 98, 242302 (2007) [nucl-ex/0610037].
• (21) B. Alver et al. [PHOBOS Collaboration], Phys. Rev. C 81, 034915 (2010) [arXiv:1002.0534 [nucl-ex]].
• (22) T. Renk and H. Niemi, Phys. Rev. C 89, 064907 (2014) [arXiv:1401.2069 [nucl-th]].
• (23) L. Yan and J. Y. Ollitrault, Phys. Rev. Lett. 112, 082301 (2014) [arXiv:1312.6555 [nucl-th]].
• (24) L. Yan, J. Y. Ollitrault and A. M. Poskanzer, Phys. Rev. C 90, 024903 (2014) [arXiv:1405.6595 [nucl-th]].
• (25) S. A. Voloshin, A. M. Poskanzer, A. Tang and G. Wang, Phys. Lett. B 659, 537 (2008) [arXiv:0708.0800 [nucl-th]].
• (26) S. A. Voloshin and A. M. Poskanzer, Phys. Lett. B 474, 27 (2000) [nucl-th/9906075].
• (27) H. J. Drescher, A. Dumitru, C. Gombeaud and J. Y. Ollitrault, Phys. Rev. C 76, 024905 (2007) [arXiv:0704.3553 [nucl-th]].
• (28) B. Alver, M. Baker, C. Loizides and P. Steinberg, arXiv:0805.4411 [nucl-ex].
• (29) B. Schenke, P. Tribedy and R. Venugopalan, Phys. Rev. C 86, 034908 (2012) [arXiv:1206.6805 [hep-ph]].
• (30) B. Schenke, P. Tribedy and R. Venugopalan, Nucl. Phys. A 926, 102 (2014) [arXiv:1312.5588 [hep-ph]].
• (31) M. L. Miller, K. Reygers, S. J. Sanders and P. Steinberg, Ann. Rev. Nucl. Part. Sci. 57, 205 (2007) [nucl-ex/0701025].
• (32) W. Broniowski, P. Bozek and M. Rybczynski, Phys. Rev. C 76, 054905 (2007) [arXiv:0706.4266 [nucl-th]].
• (33) N. Borghini, P. M. Dinh and J. Y. Ollitrault, Phys. Rev. C 64, 054901 (2001) [nucl-th/0105040].
• (34) A. Bilandzic, R. Snellings and S. Voloshin, Phys. Rev. C 83, 044913 (2011) [arXiv:1010.0233 [nucl-ex]].
• (35) G. Aad et al. [ATLAS Collaboration], Phys. Lett. B 725, 60 (2013) [arXiv:1303.2084 [hep-ex]].
• (36) B. B. Abelev et al. [ALICE Collaboration], arXiv:1406.2474 [nucl-ex].
• (37) M. Miller and R. Snellings, nucl-ex/0312008.
• (38) P. Bozek, Phys. Rev. C 85, 014911 (2012) [arXiv:1112.0915 [hep-ph]].
• (39) P. Bozek and W. Broniowski, Phys. Lett. B 718, 1557 (2013) [arXiv:1211.0845 [nucl-th]].
• (40) G. Basar and D. Teaney, arXiv:1312.6770 [nucl-th].
• (41) A. Bzdak, P. Bozek and L. McLerran, Nucl. Phys. A 927, 15 (2014) [arXiv:1311.7325 [hep-ph]].
• (42) B. Schenke and R. Venugopalan, Phys. Rev. Lett. 113, 102301 (2014) [arXiv:1405.3605 [nucl-th]].
• (43) R. S. Bhalerao, J. P. Blaizot, N. Borghini and J. Y. Ollitrault, Phys. Lett. B 627, 49 (2005) [nucl-th/0508009].
• (44) Risto Paatelainen, poster at Quark Matter 2014; Harri Niemi, plenary talk at Quark Matter 2014.
• (45) D. Teaney and L. Yan, Phys. Rev. C 86, 044908 (2012) [arXiv:1206.1905 [nucl-th]].
• (46) H. Holopainen, H. Niemi and K. J. Eskola, Phys. Rev. C 83, 034901 (2011) [arXiv:1007.0368 [hep-ph]].
• (47) F. G. Gardim, F. Grassi, M. Luzum and J. Y. Ollitrault, Phys. Rev. C 85, 024908 (2012) [arXiv:1111.6538 [nucl-th]].
• (48) A. P. Mishra, R. K. Mohapatra, P. S. Saumia and A. M. Srivastava, Phys. Rev. C 77, 064902 (2008) [arXiv:0711.1323 [hep-ph]].
• (49) K. Dusling, F. Gelis and R. Venugopalan, Nucl. Phys. A 872, 161 (2011) [arXiv:1106.3927 [nucl-th]].
• (50) J. M. Maldacena, JHEP 0305, 013 (2003) [astro-ph/0210603].
• (51) N. Bartolo, E. Komatsu, S. Matarrese and A. Riotto, Phys. Rept. 402, 103 (2004) [astro-ph/0406398].
• (52) P. A. R. Ade et al. [Planck Collaboration], arXiv:1303.5084 [astro-ph.CO].
You are adding the first comment!
How to quickly get a good reply:
• Give credit where it’s due by listing out the positive aspects of a paper before getting into which changes should be made.
• Be specific in your critique, and provide supporting evidence with appropriate references to substantiate general statements.
• Your comment should inspire ideas to flow and help the author improves the paper.

The better we are at sharing our knowledge with each other, the faster we move forward.
The feedback must be of minimum 40 characters and the title a minimum of 5 characters