$\Omega + \bar{\Omega}$ invariant mass spectra from Cu+Cu $\sqrt{s_{NN}} = 200$ GeV collisions, where $|y| < 0.5$. The uncertainties on the spectra points are statistical and systematic combined.

$K^0_S$ invariant mass spectra from Au+Au $\sqrt{s_{NN}} = 200$ GeV collisions, where $|y| < 0.5$. The uncertainties on the spectra points are statistical and systematic combined.

$\Lambda$ and $\bar{\Lambda}$ invariant mass spectra from Au+Au $\sqrt{s_{NN}} = 200$ GeV collisions, where $|y| < 0.5$. The $\Lambda$ and $\bar{\Lambda}$ yields have not been feed down subtracted from weak decays. The uncertainties on the spectra points are statistical and systematic combined.

$K^0_S$, $\Lambda$, and $\bar{\Lambda}$, spectra divided by $\langle N_{part} \rangle$ for Cu+Cu $0 − 10\%$ ($\langle N_{part} \rangle \sim 99$) and Au+Au $20 − 40\%$ ($\langle N_{part} \rangle \sim 141$) $\sqrt{s_{NN}} = 200$ GeV collisions, where $|y| < 0.5$. The $\Lambda$ and $\bar{\Lambda}$ yields have been feed down subtracted from weak decays. The uncertainties on the spectra points are statistical and systematic; for clarity the uncertainty on $\langle N_{part} \rangle$ has not been included. The curves show the functions described in the text used to extract $dN/dy$.

$\Xi + \bar{\Xi}$ spectra divided by $\langle N_{part} \rangle$ for Cu+Cu $0 − 10\%$ ($\langle N_{part} \rangle \sim 99$) $\sqrt{s_{NN}} = 200$ GeV collisions, where $|y| < 0.5$. The uncertainties on the spectra points are statistical and systematic; for clarity the uncertainty on $\langle N_{part} \rangle$ has not been included. The curves show the functions described in the text used to extract $dN/dy$.

$\Xi + \bar{\Xi}$ spectra divided by $\langle N_{part} \rangle$ for Au+Au $20 − 40\%$ ($\langle N_{part} \rangle \sim 141$) $\sqrt{s_{NN}} = 200$ GeV collisions, where $|y| < 0.5$. The uncertainties on the spectra points are statistical and systematic; for clarity the uncertainty on $\langle N_{part} \rangle$ has not been included. The curves show the functions described in the text used to extract $dN/dy$.

$\Omega + \bar{\Omega}$ spectra divided by $\langle N_{part} \rangle$ for Cu+Cu $0 − 10\%$ ($\langle N_{part} \rangle \sim 99$) $\sqrt{s_{NN}} = 200$ GeV collisions, where $|y| < 0.5$. The uncertainties on the spectra points are statistical and systematic; for clarity the uncertainty on $\langle N_{part} \rangle$ has not been included. The curves show the functions described in the text used to extract $dN/dy$.

$\Omega + \bar{\Omega}$ spectra divided by $\langle N_{part} \rangle$ for Au+Au $20 − 40\%$ ($\langle N_{part} \rangle \sim 141$) $\sqrt{s_{NN}} = 200$ GeV collisions, where $|y| < 0.5$. The uncertainties on the spectra points are statistical and systematic; for clarity the uncertainty on $\langle N_{part} \rangle$ has not been included. The curves show the functions described in the text used to extract $dN/dy$.

The enhancement factor for (multi-) strange particles in Cu+Cu $\sqrt{s_{NN}} = 200$ GeV collisions, where $|y| < 0.5$. The $\Lambda$, and $\bar{\Lambda}$ yields have been feed-down subtracted in all cases. The black bars show the normalization uncertainties, and the uncertainties for the heavy-ion points are the combined statistical and systematic errors. Curves described in the text, where $B_{K} = 2.0$, $B_{\Lambda} = 2.4$, $B_{\Xi} = 5.0$ and $B_{\Omega} = 12.1$.

The enhancement factor for (multi-) strange particles in Au+Au $\sqrt{s_{NN}} = 200$ GeV collisions, where $|y| < 0.5$. The $\Lambda$, and $\bar{\Lambda}$ yields have been feed-down subtracted in all cases. The black bars show the normalization uncertainties, and the uncertainties for the heavy-ion points are the combined statistical and systematic errors. Curves described in the text, where $B_{K} = 2.0$, $B_{\Lambda} = 2.4$, $B_{\Xi} = 5.0$ and $B_{\Omega} = 12.1$.

Ratio of particle yields in central Cu+Cu and midcentral Au+Au collisions when $\langle N_{part} \rangle = 99$ in each case for $|y| < 0.5$. $\pi$ yields are from elsewhere [17]. Boxed uncertainties are from the Glauber calculations and are correlated for every particle. $\langle N_{part>1} \rangle$ refers to the parameterization shown by eq. 1, while the EPOS and AMPT models are described in the text. The default settings are used for each model. The vertical lines show the remaining independent statistical and systematic uncertainties.

$\rho^0$ production cross section determined with the data set collected with trigger B, as a function of momentum transfer $t$, fitted with a double exponential fit function in the range $t < 0.1$. The statistical errors are shown. The ratio of incoherent to coherent cross sections is measured to be $0.20 \pm 0.8$. The fit parameters are shown in Table I.

Comparison of theoretical predictions to the measured total cross section for coherent $\rho^0$ production as a functionof $\sqrt{s_{NN}}$ . The measured cross section is based on the dataset collected with trigger B. The error bars show the sum of the statistical and systematic uncertainties. See text for details.

Differential cross section for the process GAMMA P --> PI0 P as a function of the cosine of the centre-of-mass scattering angle of the PI0 for photon energies from 0.925 to 0.950 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the cosine of the centre-of-mass scattering angle of the PI0 for photon energies from 0.950 to 0.975 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the cosine of the centre-of-mass scattering angle of the PI0 for photon energies from 0.975 to 1.000 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the cosine of the centre-of-mass scattering angle of the PI0 for photon energies from 1.000 to 1.025 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the cosine of the centre-of-mass scattering angle of the PI0 for photon energies from 1.025 to 1.050 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the cosine of the centre-of-mass scattering angle of the PI0 for photon energies from 1.050 to 1.075 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the cosine of the centre-of-mass scattering angle of the PI0 for photon energies from 1.100 to 1.125 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the cosine of the centre-of-mass scattering angle of the PI0 for photon energies from 1.125 to 1.150 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the cosine of the centre-of-mass scattering angle of the PI0 for photon energies from 1.150 to 1.175 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the cosine of the centre-of-mass scattering angle of the PI0 for photon energies from 1.175 to 1.200 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the cosine of the centre-of-mass scattering angle of the PI0 for photon energies from 1.200 to 1.225 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the cosine of the centre-of-mass scattering angle of the PI0 for photon energies from 1.225 to 1.250 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the cosine of the centre-of-mass scattering angle of the PI0 for photon energies from 1.250 to 1.275 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the cosine of the centre-of-mass scattering angle of the PI0 for photon energies from 1.275 to 1.300 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the cosine of the centre-of-mass scattering angle of the PI0 for photon energies from 1.300 to 1.350 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the cosine of the centre-of-mass scattering angle of the PI0 for photon energies from 1.350 to 1.400 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the cosine of the centre-of-mass scattering angle of the PI0 for photon energies from 1.400 to 1.450 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the cosine of the centre-of-mass scattering angle of the PI0 for photon energies from 1.450 to 1.500 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the cosine of the centre-of-mass scattering angle of the PI0 for photon energies from 1.500 to 1.550 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the cosine of the centre-of-mass scattering angle of the PI0 for photon energies from 1.550 to 1.600 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the cosine of the centre-of-mass scattering angle of the PI0 for photon energies from 1.600 to 1.650 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the cosine of the centre-of-mass scattering angle of the PI0 for photon energies from 1.650 to 1.700 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the cosine of the centre-of-mass scattering angle of the PI0 for photon energies from 1.700 to 1.750 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the cosine of the centre-of-mass scattering angle of the PI0 for photon energies from 1.750 to 1.800 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the cosine of the centre-of-mass scattering angle of the PI0 for photon energies from 1.800 to 1.850 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the cosine of the centre-of-mass scattering angle of the PI0 for photon energies from 1.850 to 1.900 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the cosine of the centre-of-mass scattering angle of the PI0 for photon energies from 1.900 to 1.950 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the cosine of the centre-of-mass scattering angle of the PI0 for photon energies from 1.950 to 2.000 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the cosine of the centre-of-mass scattering angle of the PI0 for photon energies from 2.000 to 2.050 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the cosine of the centre-of-mass scattering angle of the PI0 for photon energies from 2.050 to 2.100 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the cosine of the centre-of-mass scattering angle of the PI0 for photon energies from 2.100 to 2.150 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the cosine of the centre-of-mass scattering angle of the PI0 for photon energies from 2.150 to 2.200 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the cosine of the centre-of-mass scattering angle of the PI0 for photon energies from 2.200 to 2.250 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the cosine of the centre-of-mass scattering angle of the PI0 for photon energies from 2.250 to 2.300 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the cosine of the centre-of-mass scattering angle of the PI0 for photon energies from 2.300 to 2.350 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the cosine of the centre-of-mass scattering angle of the PI0 for photon energies from 2.350 to 2.400 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the cosine of the centre-of-mass scattering angle of the PI0 for photon energies from 2.400 to 2.450 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the cosine of the centre-of-mass scattering angle of the PI0 for photon energies from 2.450 to 2.500 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the scattering angle of the PI0 for photon energies from 0.850 to 0.875 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the scattering angle of the PI0 for photon energies from 0.875 to 0.900 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the scattering angle of the PI0 for photon energies from 0.900 to 0.925 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the scattering angle of the PI0 for photon energies from 0.925 to 0.950 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the scattering angle of the PI0 for photon energies from 0.950 to 0.975 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the scattering angle of the PI0 for photon energies from 0.975 to 1.000 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the scattering angle of the PI0 for photon energies from 1.000 to 1.025 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the scattering angle of the PI0 for photon energies from 1.025 to 1.050 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the scattering angle of the PI0 for photon energies from 1.050 to 1.075 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the scattering angle of the PI0 for photon energies from 1.100 to 1.125 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the scattering angle of the PI0 for photon energies from 1.125 to 1.150 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the scattering angle of the PI0 for photon energies from 1.150 to 1.175 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the scattering angle of the PI0 for photon energies from 1.175 to 1.200 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the scattering angle of the PI0 for photon energies from 1.200 to 1.225 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the scattering angle of the PI0 for photon energies from 1.225 to 1.250 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the scattering angle of the PI0 for photon energies from 1.250 to 1.275 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the scattering angle of the PI0 for photon energies from 1.275 to 1.300 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the scattering angle of the PI0 for photon energies from 1.300 to 1.350 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the scattering angle of the PI0 for photon energies from 1.350 to 1.400 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the scattering angle of the PI0 for photon energies from 1.400 to 1.450 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the scattering angle of the PI0 for photon energies from 1.450 to 1.500 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the scattering angle of the PI0 for photon energies from 1.500 to 1.550 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the scattering angle of the PI0 for photon energies from 1.550 to 1.600 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the scattering angle of the PI0 for photon energies from 1.600 to 1.650 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the scattering angle of the PI0 for photon energies from 1.650 to 1.700 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the scattering angle of the PI0 for photon energies from 1.700 to 1.750 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the scattering angle of the PI0 for photon energies from 1.750 to 1.800 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the scattering angle of the PI0 for photon energies from 1.800 to 1.850 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the scattering angle of the PI0 for photon energies from 1.850 to 1.900 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the scattering angle of the PI0 for photon energies from 1.900 to 1.950 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the scattering angle of the PI0 for photon energies from 1.950 to 2.000 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the scattering angle of the PI0 for photon energies from 2.000 to 2.050 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the scattering angle of the PI0 for photon energies from 2.050 to 2.100 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the scattering angle of the PI0 for photon energies from 2.100 to 2.150 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the scattering angle of the PI0 for photon energies from 2.150 to 2.200 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the scattering angle of the PI0 for photon energies from 2.200 to 2.250 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the scattering angle of the PI0 for photon energies from 2.250 to 2.300 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the scattering angle of the PI0 for photon energies from 2.300 to 2.350 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the scattering angle of the PI0 for photon energies from 2.350 to 2.400 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the scattering angle of the PI0 for photon energies from 2.400 to 2.450 GeV.

Differential cross section for the process GAMMA P --> PI0 P as a function of the scattering angle of the PI0 for photon energies from 2.450 to 2.500 GeV.

Inclusive jet double-differential cross section as a function of jet transverse momentum in the |rapidity| range 1.5 to 2.0 using an anti-kT jet resolution parameter R of 0.5.

Inclusive jet double-differential cross section as a function of jet transverse momentum in the |rapidity| range 2.0 to 2.5 using an anti-kT jet resolution parameter R of 0.5.

Inclusive jet double-differential cross section as a function of jet transverse momentum in the |rapidity| range 2.5 to 3.0 using an anti-kT jet resolution parameter R of 0.5.

Candidate estimated mass distribitions for data, expected background with error and simulated signals for the R-hadron search.

The expected production cross section for GMSB events with N_5=3, m_messenger=250 TeV, sign(mu)=1 and tan(beta)=5 and the observed cross section 95% CL upper limit as a funtion of the stau mass for the slepton search.

The expected production cross section for GMSB events for electroweak processes only and the observed cross section 95% CL upper limit as a funtion of the stau mass for the slepton search.

The expected production cross-section for R-hadron events and the 95% CL limit as a function of the gluino mass and for different gluino-ball fractions. Also shown are the 1 sig limits for the 0.1 gluino-ball fraction.RE = P P --> R-HADRON X.

Diphoton production cross section as a function of the diphoton rapidity.

Diphoton production cross section differential in the cosine of the polar angle in the Collins-Soper frame.

Diphoton production cross section differential in the sub-leading to leading photon transverse momentum ratio (z).

The correlation function C, C is plotted in units of (GeV/c)$^2$ and the relative azimuthal angle ∆φ in radians for 30-40% centrality in Au+Au collisions at $\sqrt{s_{NN}}$ = 200 GeV. Relative statistical errors range from 0.8% in peripheral collisions to 0.9% in the most central collisions at the peak of the distribution.

The correlation function C, C is plotted in units of (GeV/c)$^2$ and the relative azimuthal angle ∆φ in radians for 0-5% centrality in Au+Au collisions at $\sqrt{s_{NN}}$ = 200 GeV..Relative statistical errors range from 0.8% in peripheral collisions to 0.9% in the most central collisions at the peak of the distribution.

The correlation function C, C is plotted in units of (GeV/c)$^2$ and the relative azimuthal angle ∆φ in radians for 0-5% centrality in Au+Au collisions at $\sqrt{s_{NN}}$ = 200 GeV..Relative statistical errors range from 0.8% in peripheral collisions to 0.9% in the most central collisions at the peak of the distribution.

Projection of the correlation function C, for|∆φ|<1.0 radians on the ∆η axis for 70-80% centrality in Au+Au collisions at $\sqrt{s_{NN}}$ = 200 GeV. The correlation function C is plottedin units of (GeV/c)$^2$.The correlation function C is plotted in units of (GeV/c)$^2$. The solid line shows the fit obtained with Eq.2. The dotted line corresponds to the baseline, b, obtained in the fit and shaded band shows uncertainty in determining b.

Projection of the correlation function C, for|∆φ|<1.0 radians on the ∆η axis for 70-80% centrality in Au+Au collisions at $\sqrt{s_{NN}}$ = 200 GeV. The correlation function C is plottedin units of (GeV/c)$^2$.The correlation function C is plotted in units of (GeV/c)$^2$. The solid line shows the fit obtained with Eq.2. The dotted line corresponds to the baseline, b, obtained in the fit and shaded band shows uncertainty in determining b.

Projection of the correlation function C, for|∆φ|<1.0 radians on the ∆η axis for 30-40% centrality. Statistical errors at(\Deltaeta_1,Deltaeta_2~(0,0) are approximately 0.084 for Au+Au. The correlation function C is plotted in units of (GeV/c)$^2$. The dotted line corresponds to the baseline,b, obtained in the fit and shaded band shows uncertainty in determining b.

Projection of the correlation function C, for|∆φ|<1.0 radians on the ∆η axis for 30-40% centrality. Statistical errors at(\Deltaeta_1,Deltaeta_2~(0,0) are approximately 0.084 for Au+Au. The correlation function C is plotted in units of (GeV/c)$^2$. The dotted line corresponds to the baseline,b, obtained in the fit and shaded band shows uncertainty in determining b.

Projection of the correlation function C, for|∆φ|<1.0 radians on the ∆η axis for 0-5% centrality in Au+Au collisions at $\sqrt{s_{NN}}$ = 200 GeV. The correlation functionCis plotted in units of (GeV/c)$^2$. The correlation function C is plotted in units of (GeV/c)$^2$. The solid line shows the fit obtained with Eq.2. The dotted line corresponds to the baseline,b, obtained in the fit and shaded band shows uncertainty in determining b.

Projection of the correlation function C, for|∆φ|<1.0 radians on the ∆η axis for 0-5% centrality in Au+Au collisions at $\sqrt{s_{NN}}$ = 200 GeV. The correlation functionCis plotted in units of (GeV/c)$^2$. The correlation function C is plotted in units of (GeV/c)$^2$. The solid line shows the fit obtained with Eq.2. The dotted line corresponds to the baseline,b, obtained in the fit and shaded band shows uncertainty in determining b.

RMS as function of the number of participating nucleons for the correlation function C, for nine centrality classes in Au+Au collisions at $\sqrt{s_{NN}}$ = 200 GeV. The dotted line represents a lower limit estimate of the RMS explained in the text and the shaded band represents systematic uncertainties on the RMS.

RMS as function of the number of participating nucleons for the correlation function C, for nine centrality classes in Au+Au collisions at $\sqrt{s_{NN}}$ = 200 GeV. The dotted line represents a lower limit estimate of the RMS explained in the text and the shaded band represents systematic uncertainties on the RMS.

Total J/PSI cross section from the di-electron data. The first error is statistical, the second is a systematic error. The second systematic errors is related to the unknown polarization. Only the one from the Helicity Frame is quoted here. It has the biggest influence in this rapidity range. Data updated from the erratum.

Total J/PSI cross section from the di-muon data. The first error is statistical, the second is a systematic error. The second systematic errors is related to the unknown polarization. Only the one from the Collins Soper Frame is quoted here. It has the biggest influence in this rapidity range.