Same charge C3 and c3 in Pb Pb collisions projected against Q3.

Mixed charge C3 and c3 in pp collisions projected against Q3.

Mixed charge C3 and c3 in p Pb collisions projected against Q3.

Mixed charge C3 and c3 in Pb Pb collisions projected against Q3.

Gaussian radii and intercept parameters in pp collisions versus Nch at low KT3.

Gaussian radii and intercept parameters in pPb collisions versus Nch at low KT3.

Gaussian radii and intercept parameters in PbPb collisions versus Nch at low KT3.

Gaussian radii and intercept parameters in pp collisions versus Nch at high KT3.

Gaussian radii and intercept parameters in pPb collisions versus Nch at high KT3.

Gaussian radii and intercept parameters in PbPb collisions versus Nch at high KT3.

Edgeworth radii and intercept parameters in pp collisions versus Nch at low KT3.

Edgeworth radii and intercept parameters in pPb collisions versus Nch at low KT3.

Edgeworth radii and intercept parameters in PbPb collisions versus Nch at low KT3.

Edgeworth radii and intercept parameters in pp collisions versus Nch at high KT3.

Edgeworth radii and intercept parameters in pPb collisions versus Nch at high KT3.

Edgeworth radii and intercept parameters in PbPb collisions versus Nch at high KT3.

Exponential radii scaled down by sqrt(pi) and intercept parameters in pp collisions versus Nch at low KT3.

Exponential radii scaled down by sqrt(pi) and intercept parameters in pPb collisions versus Nch at low KT3.

Exponential radii scaled down by sqrt(pi) and intercept parameters in PbPb collisions versus Nch at low KT3.

Exponential radii scaled down by sqrt(pi) and intercept parameters in pp collisions versus Nch at high KT3.

Exponential radii scaled down by sqrt(pi) and intercept parameters in pPb collisions versus Nch at high KT3.

Exponential radii scaled down by sqrt(pi) and intercept parameters in PbPb collisions versus Nch at high KT3.

c3 comparison between pp and pPb collisions at similar multiplicity.

c3 comparison between pB and PbPb collisions at similar multiplicity.

The total coherent $\mathrm{J}/\psi$ photoproduction cross section as a function of photon-nuclear center-of-mass energy per nucleon $W_{\gamma \mathrm{N}}^{\mathrm{Pb}}$, measured in PbPb ultra-peripheral collisions at $\sqrt{s_{\mathrm{NN}}}$ = 5.02 TeV. The $W_{\gamma \mathrm{N}}^{\mathrm{Pb}}$ values used correspond to the center of each rapidity range. The theoretical uncertainties is due to the uncertainties in the photon flux.

The nuclear gluon suppression factor $R_{\mathrm{g}}^{\mathrm{Pb}}$ as a function of Bjorken $x$ extracted from the CMS measurement of the coherent $\mathrm{J}/\psi$ photoproduction in PbPb ultra-peripheral collisions at $\sqrt{s_{\mathrm{NN}}}$ = 5.02 TeV. The $x$ values are evaluated at the centers of their corresponding rapidity ranges. The theoretical uncertainties are due to the uncertainties in the photon flux and the impulse approximation model.

The nuclear gluon suppression factor $R_{\mathrm{g}}^{\mathrm{Pb}}$ as a function of Bjorken $x$ extracted from the CMS measurement of the coherent $\mathrm{J}/\psi$ photoproduction in PbPb ultra-peripheral collisions at $\sqrt{s_{\mathrm{NN}}}$ = 5.02 TeV. The $x$ values are evaluated at the centers of their corresponding rapidity ranges. The theoretical uncertainties are due to the uncertainties in the photon flux and the impulse approximation model.

The total covariance matrix of the total coherent photoproduction cross section as a function of photon-nuclear center-of-mass energy per nucleon $W_{\gamma \mathrm{N}}^{\mathrm{Pb}}$. The covariance matrix includes both the experimental and theoretical (photon flux) uncertainties. The bins are ordered as increasing in $W_{\gamma \mathrm{N}}^{\mathrm{Pb}}$.

The photon flux values from STARLight as a function of rapidity, in different neutron multiplicity classes: 0n0n, 0nXn, and XnXn.

The experimental covariance matrix of the total coherent photoproduction cross section as a function of photon-nuclear center-of-mass energy per nucleon $W_{\gamma \mathrm{N}}^{\mathrm{Pb}}$. The bins are ordered as increasing in $W_{\gamma \mathrm{N}}^{\mathrm{Pb}}$.

The covariance matrix for the flux in the 0n0n neutron multiplicity class.

The theoretical (photon flux) covariance matrix of the total coherent photoproduction cross section as a function of photon-nuclear center-of-mass energy per nucleon $W_{\gamma \mathrm{N}}^{\mathrm{Pb}}$. The bins are ordered as increasing in $W_{\gamma \mathrm{N}}^{\mathrm{Pb}}$.

The covariance matrix for the flux in the 0nXn neutron multiplicity class.

The covariance matrix for the flux in the XnXn neutron multiplicity class.

The total covariance matrix of the total coherent photoproduction cross section as a function of photon-nuclear center-of-mass energy per nucleon $W_{\gamma \mathrm{N}}^{\mathrm{Pb}}$. The covariance matrix includes both the experimental and theoretical (photon flux) uncertainties. The bins are ordered as increasing in $W_{\gamma \mathrm{N}}^{\mathrm{Pb}}$.

The experimental covariance matrix of the total coherent photoproduction cross section as a function of photon-nuclear center-of-mass energy per nucleon $W_{\gamma \mathrm{N}}^{\mathrm{Pb}}$. The bins are ordered as increasing in $W_{\gamma \mathrm{N}}^{\mathrm{Pb}}$.

The theoretical (photon flux) covariance matrix of the total coherent photoproduction cross section as a function of photon-nuclear center-of-mass energy per nucleon $W_{\gamma \mathrm{N}}^{\mathrm{Pb}}$. The bins are ordered as increasing in $W_{\gamma \mathrm{N}}^{\mathrm{Pb}}$.