Measured $\frac{d\sigma}{d(-t^{\prime})}~[\mathrm{nb/GeV^{2}}]$ for reaction $\gamma p\to \{\Lambda \bar{\Lambda}\} p$ including data of $6.5 \leq E_{\gamma} \leq 11.5$ [GeV], splitted in 10 energy bins (each as a column in the table). The observable $(-t^{\prime})$ is in unit of $[\mathrm{nb/GeV^{2}}]$ and is divided into bins of width 0.03 $[\mathrm{GeV^{2}}]$ (each as a row in the table). The global systematic uncertainty is 19% (not included in the table), with contributions of 5% from kinematic fitting, 10% from data selection, 5% from flux normalization, 13% from tracking efficiency, 3% from model dependence, and 6% from run-period variations.

Measured $\frac{d\sigma}{d(-t^{\prime})}~[\mathrm{nb/GeV^{2}}]$ for reaction $\gamma p\to \{p \bar{\Lambda}\} \Lambda$ including data of $6.5 \leq E_{\gamma} \leq 11.5$ [GeV], splitted in 10 energy bins (each as a column in the table). The observable $(-t^{\prime})$ is in unit of $[\mathrm{nb/GeV^{2}}]$ and is divided into bins of width 0.075 $[\mathrm{GeV^{2}}]$ (each as a row in the table). The global systematic uncertainty is 22% (not included in the table), with contributions of 2% from kinematic fitting, 10% from data selection, 5% from flux normalization, 15% from tracking efficiency, 3% from model dependence, and 10% from run-period variations.

Measured $\frac{d\sigma}{d(-t^{\prime})}~[\mathrm{nb/GeV^{2}}]$ for reaction $\gamma p\to \{p \bar{p}\} p$ including data of $6.5 \leq E_{\gamma} \leq 11.5$ [GeV], splitted in 10 energy bins (each as a column in the table). The observable $(-t^{\prime})$ is in unit of $[\mathrm{nb/GeV^{2}}]$ and is divided into bins of width 0.01 $[\mathrm{GeV^{2}}]$ (each as a row in the table). The global systematic uncertainty is 13% (not included in the table), with contributions of 8% from kinematic fitting, 4% from data selection, 5% from flux normalization, 8% from tracking efficiency, 3% from model dependence, and 1% from run-period variations.

Measured $\frac{d\sigma}{d(-t^{\prime})}~[\mathrm{nb/GeV^{2}}]$ for reaction $\gamma p\to \{p \bar{p}\} p$ including data of $3.5 \leq E_{\gamma} \leq 6.0$ [GeV], splitted in 5 energy bins (each as a column in the table). The observable $(-t^{\prime})$ is in unit of $[\mathrm{nb/GeV^{2}}]$ and is divided into bins of width 0.1 $[\mathrm{GeV^{2}}]$ (each as a row in the table). The global systematic uncertainty is 13% (not included in the table), with contributions of 8% from kinematic fitting, 4% from data selection, 5% from flux normalization, 8% from tracking efficiency, 3% from model dependence, and 1% from run-period variations.

Measured total cross section $\sigma(\gamma\,p\to\{\Lambda\bar{\Lambda}\}p)$ in unit of [nb] with beam energy in the range $5.0 < E_{\gamma} < 11.5~[\mathrm{GeV}]$ with various bin width. The table only includes point-to-point statistical uncertainties. The global systematic uncertainty is 19% (not included in the table), with contributions of 5% from kinematic fitting, 10% from data selection, 5% from flux normalization, 13% from tracking efficiency, 3% from model dependence, and 6% from run-period variations.

Measured total cross section $\sigma(\gamma\,p\to\{p\bar{\Lambda}\}\Lambda)$ in unit of [nb] with beam energy in the range $5.0 < E_{\gamma} < 11.5~[\mathrm{GeV}]$ with various bin width. The table only includes point-to-point statistical uncertainties. The global systematic uncertainty is 22% (not included in the table), with contributions of 2% from kinematic fitting, 10% from data selection, 5% from flux normalization, 15% from tracking efficiency, 3% from model dependence, and 10% from run-period variations.

Measured total cross section $\sigma(\gamma\,p\to\{p\bar{p}\}p)$ in unit of [nb] with beam energy in the range $3.5 < E_{\gamma} < 11.5~[\mathrm{GeV}]$ with various bin width. The table only includes point-to-point statistical uncertainties. The global systematic uncertainty is 13% (not included in the table), with contributions of 8% from kinematic fitting, 4% from data selection, 5% from flux normalization, 8% from tracking efficiency, 3% from model dependence, and 1% from run-period variations.

Single Event Sensitivity (SES) for the $K^{+}\rightarrow\pi^{+}X$ search as a function of X mass.

Model-independent constraints on the branching ratio of the $K^{+}\rightarrow\pi^{+}X$ decay

Model-independent constraints on the branching ratio of the $K^{+}\rightarrow\pi^{+}X$ decay

Observed model-independent upper limits at 90 % CL of $\mathcal{B}(K^{+}\rightarrow\pi^{+}X)$ as function of $X$ mass, for several $X$ lifetime hypotheses, assuming $X$ decays to visible SM particles.

Observed model-independent upper limits at 90 % CL of $\mathcal{B}(K^{+}\rightarrow\pi^{+}X)$ as function of $X$ mass, for several $X$ lifetime hypotheses, assuming $X$ decays to visible SM particles.

Di-muon mass spectrum of selected $K^{+}\rightarrow\pi^{+}\mu^{+}\mu^{-}$ events from 2017–2018 data.

Di-muon mass spectrum of selected $K^{+}\rightarrow\pi^{+}\mu^{+}\mu^{-}$ events from 2017–2018 data.

Expected and observed model-independent upper limits at 90 % CL for $\mathcal{B}(K^{+}\rightarrow\pi^{+}X)\times\mathcal{B}(X\rightarrow\mu^{+}\mu^{-})$ as a function of $m_{X}$ for $\tau_{X}=0$.

Expected and observed model-independent upper limits at 90 % CL for $\mathcal{B}(K^{+}\rightarrow\pi^{+}X)\times\mathcal{B}(X\rightarrow\mu^{+}\mu^{-})$ as a function of $m_{X}$ for $\tau_{X}=0$.

Observed model-independent upper limits at 90 % CL for $\mathcal{B}(K^{+}\rightarrow\pi^{+}X)\times\mathcal{B}(X\rightarrow\mu^{+}\mu^{-})$ for several $\tau_{X}$ values.

Observed model-independent upper limits at 90 % CL for $\mathcal{B}(K^{+}\rightarrow\pi^{+}X)\times\mathcal{B}(X\rightarrow\mu^{+}\mu^{-})$ for several $\tau_{X}$ values.

Branching ratio of the $K^{+}\rightarrow\pi^{+}A^{\prime}$ decay divided by the kinetic mixing coupling squared, $\varepsilon^{2}$, as a function of $m_{A^{\prime}}$ for the BC2 model with dark photon $A^{\prime}$.

Branching ratio of the $K^{+}\rightarrow\pi^{+}A^{\prime}$ decay divided by the kinetic mixing coupling squared, $\varepsilon^{2}$, as a function of $m_{A^{\prime}}$ for the BC2 model with dark photon $A^{\prime}$.

Excluded region, at 90 % CL, of the parameter space $(m_{A^{\prime}},\varepsilon)$ for a dark photon $A^{\prime}$, decaying invisibly, in the BC2 model for the NA62 $K^{+}\rightarrow\pi^{+}X_{\rm inv}$ search.

Excluded region, at 90 % CL, of the parameter space $(m_{A^{\prime}},\varepsilon)$ for a dark photon $A^{\prime}$, decaying invisibly, in the BC2 model for the NA62 $K^{+}\rightarrow\pi^{+}X_{\rm inv}$ search.

Excluded region, at 90 % CL, of the parameter space $(m_{A^{\prime}},\varepsilon)$ for a dark photon $A^{\prime}$, decaying invisibly, in the BC2 model for the NA62 $\pi^{0}\rightarrow{\rm inv}$ search.

Excluded region, at 90 % CL, of the parameter space $(m_{A^{\prime}},\varepsilon)$ for a dark photon $A^{\prime}$, decaying invisibly, in the BC2 model for the NA62 $\pi^{0}\rightarrow{\rm inv}$ search.

Branching ratio of the $K^{+}\rightarrow\pi^{+}S$ decay divided by $\text{sin}^{2}\theta$, as a function of $m_{S}$.

Branching ratio of the $K^{+}\rightarrow\pi^{+}S$ decay divided by $\text{sin}^{2}\theta$, as a function of $m_{S}$.

Excluded regions, at 90 % CL, of the parameter space $(m_{S},\rm{sin}^{2}\theta)$ for a dark scalar $S$, in the BC4-inv model for the NA62 $K^{+}\rightarrow\pi^{+}X_{\rm inv}$ search.

Excluded regions, at 90 % CL, of the parameter space $(m_{S},\rm{sin}^{2}\theta)$ for a dark scalar $S$, in the BC4-inv model for the NA62 $K^{+}\rightarrow\pi^{+}X_{\rm inv}$ search.

Excluded regions, at 90 % CL, of the parameter space $(m_{S},\rm{sin}^{2}\theta)$ for a dark scalar $S$, in the BC4-inv model for the NA62 $\pi^{0}\rightarrow{\rm inv}$ search.

Excluded regions, at 90 % CL, of the parameter space $(m_{S},\rm{sin}^{2}\theta)$ for a dark scalar $S$, in the BC4-inv model for the NA62 $\pi^{0}\rightarrow{\rm inv}$ search.

Excluded regions, at 90 % CL, of the parameter space $(m_{S},\rm{sin}^{2}\theta$) for a dar scalar S, in the BC4 model, from the NA62 $K^{+}\rightarrow\pi^{+}X_{\rm inv}$ search.

Excluded regions, at 90 % CL, of the parameter space $(m_{S},\rm{sin}^{2}\theta$) for a dar scalar S, in the BC4 model, from the NA62 $K^{+}\rightarrow\pi^{+}X_{\rm inv}$ search.

Excluded regions, at 90 % CL, of the parameter space $(m_{S},\rm{sin}^{2}\theta$) for a dar scalar S, in the BC4 model, from the NA62 $K^{+}\rightarrow\pi^{+}\mu^{+}\mu^{-}$ study.

Excluded regions, at 90 % CL, of the parameter space $(m_{S},\rm{sin}^{2}\theta$) for a dar scalar S, in the BC4 model, from the NA62 $K^{+}\rightarrow\pi^{+}\mu^{+}\mu^{-}$ study.

Branching ratio of the $K^{+}\rightarrow\pi^{+}a$ decay divided by $(C_{ff}/\Lambda)^{2}$, as a function of $m_{a}$, assuming Λ = 1 TeV.

Branching ratio of the $K^{+}\rightarrow\pi^{+}a$ decay divided by $(C_{ff}/\Lambda)^{2}$, as a function of $m_{a}$, assuming Λ = 1 TeV.

Excluded regions, at 90 % CL, of the parameter space $(m_{a}, C_{ff}/\Lambda)$ for an ALP $a$, in the BC10-inv model, evaluated assuming $\Lambda = 1$ TeV, for the NA62 $K^{+}\rightarrow\pi^{+}X_{\rm inv}$ search.

Excluded regions, at 90 % CL, of the parameter space $(m_{a}, C_{ff}/\Lambda)$ for an ALP $a$, in the BC10-inv model, evaluated assuming $\Lambda = 1$ TeV, for the NA62 $K^{+}\rightarrow\pi^{+}X_{\rm inv}$ search.

Excluded regions, at 90 % CL, of the parameter space $(m_{a}, C_{ff}/\Lambda)$ for an ALP $a$, in the BC10-inv model, evaluated assuming $\Lambda = 1$ TeV, for the NA62 $\pi^{0}\rightarrow\rm{inv}$ search.

Excluded regions, at 90 % CL, of the parameter space $(m_{a}, C_{ff}/\Lambda)$ for an ALP $a$, in the BC10-inv model, evaluated assuming $\Lambda = 1$ TeV, for the NA62 $\pi^{0}\rightarrow\rm{inv}$ search.

Excluded regions, at 90 % CL, of the parameter space $(m_{a}, C_{ff}/\lambda)$ for an ALP $a$, in the BC10 model, evaluated assuming $\Lambda = 1$ TeV for the NA62 $K^{+}\rightarrow\pi^{+}X_{\rm inv}$ search.

Excluded regions, at 90 % CL, of the parameter space $(m_{a}, C_{ff}/\lambda)$ for an ALP $a$, in the BC10 model, evaluated assuming $\Lambda = 1$ TeV for the NA62 $K^{+}\rightarrow\pi^{+}X_{\rm inv}$ search.

Excluded regions, at 90 % CL, of the parameter space $(m_{a}, C_{ff}/\lambda)$ for an ALP $a$, in the BC10 model, evaluated assuming $\Lambda = 1$ TeV for the NA62 $\pi^{0}\rightarrow\rm{inv}$ search.

Excluded regions, at 90 % CL, of the parameter space $(m_{a}, C_{ff}/\lambda)$ for an ALP $a$, in the BC10 model, evaluated assuming $\Lambda = 1$ TeV for the NA62 $\pi^{0}\rightarrow\rm{inv}$ search.

Excluded regions, at 90 % CL, of the parameter space $(m_{a}, C_{ff}/\lambda)$ for an ALP $a$, in the BC10 model, evaluated assuming $\Lambda = 1$ TeV for the NA62 $K^{+}\rightarrow\pi^{+}\mu^{+}\mu^{-}$ study.

Excluded regions, at 90 % CL, of the parameter space $(m_{a}, C_{ff}/\lambda)$ for an ALP $a$, in the BC10 model, evaluated assuming $\Lambda = 1$ TeV for the NA62 $K^{+}\rightarrow\pi^{+}\mu^{+}\mu^{-}$ study.

Branching ratio of the $K^{+}\rightarrow\pi^{+}a$ decay divided by $(C_{GG}/\Lambda)^{2}$, as a function of $m_{a}$, assuming $\Lambda = 1$ TeV.

Branching ratio of the $K^{+}\rightarrow\pi^{+}a$ decay divided by $(C_{GG}/\Lambda)^{2}$, as a function of $m_{a}$, assuming $\Lambda = 1$ TeV.

Excluded regions, at 90 % CL, of the parameter space $(m_{a}, C_{GG}/\Lambda)$ for an ALP $a$, of the BC11 model, evaluated assuming $\Lambda = 1$ TeV, from the NA62 search for $K^{+}\rightarrow\pi^{+}X_{\rm inv}$.

Excluded regions, at 90 % CL, of the parameter space $(m_{a}, C_{GG}/\Lambda)$ for an ALP $a$, of the BC11 model, evaluated assuming $\Lambda = 1$ TeV, from the NA62 search for $K^{+}\rightarrow\pi^{+}X_{\rm inv}$.

Excluded regions, at 90 % CL, of the parameter space $(m_{a}, C_{GG}/\Lambda)$ for an ALP $a$, of the BC11 model, evaluated assuming $\Lambda = 1$ TeV, from the NA62 search for $\pi^{0}\rightarrow\rm{inv}$.

Excluded regions, at 90 % CL, of the parameter space $(m_{a}, C_{GG}/\Lambda)$ for an ALP $a$, of the BC11 model, evaluated assuming $\Lambda = 1$ TeV, from the NA62 search for $\pi^{0}\rightarrow\rm{inv}$.

Excluded regions, at 90 % CL, of the parameter space $(m_{a}, C_{GG}/\Lambda)$ for an ALP $a$, of the BC11 model, evaluated assuming $\Lambda = 1$ TeV, from the NA62 $K^{+}\rightarrow\pi^{+}\gamma\gamma$ study.

Excluded regions, at 90 % CL, of the parameter space $(m_{a}, C_{GG}/\Lambda)$ for an ALP $a$, of the BC11 model, evaluated assuming $\Lambda = 1$ TeV, from the NA62 $K^{+}\rightarrow\pi^{+}\gamma\gamma$ study.

Collins asymmetries, $A_{\mathrm{UT}}^{\sin(\phi_S - \phi_H)}$, as a function of $\pi^{-}$ momentum fraction longitudinal momentum fraction $z$ in $p^{\uparrow}p$ collisions at $\sqrt{s} = 510$ GeV. Vertical bars show the statistical uncertainties; boxes show the systematic uncertainties.

Collins asymmetries, $A_{\mathrm{UT}}^{\sin(\phi_S - \phi_H)}$, as a function of the $\pi^{+}$ momentum transverse to the jet axis, $j_{\mathrm{T}}$ with 0.1 < $z$ < 0.2

Collins asymmetries, $A_{\mathrm{UT}}^{\sin(\phi_S - \phi_H)}$, as a function of the $\pi^{-}$ momentum transverse to the jet axis, $j_{\mathrm{T}}$ with 0.1 < $z$ < 0.2

Collins asymmetries, $A_{\mathrm{UT}}^{\sin(\phi_S - \phi_H)}$, as a function of the $\pi^{+}$ momentum transverse to the jet axis, $j_{\mathrm{T}}$ with 0.2 < $z$ < 0.3

Collins asymmetries, $A_{\mathrm{UT}}^{\sin(\phi_S - \phi_H)}$, as a function of the $\pi^{-}$ momentum transverse to the jet axis, $j_{\mathrm{T}}$ with 0.2 < $z$ < 0.3

Collins asymmetries, $A_{\mathrm{UT}}^{\sin(\phi_S - \phi_H)}$, as a function of the $\pi^{+}$ momentum transverse to the jet axis, $j_{\mathrm{T}}$ with 0.3 < $z$ < 0.4

Collins asymmetries, $A_{\mathrm{UT}}^{\sin(\phi_S - \phi_H)}$, as a function of the $\pi^{-}$ momentum transverse to the jet axis, $j_{\mathrm{T}}$ with 0.3 < $z$ < 0.4

Collins asymmetries, $A_{\mathrm{UT}}^{\sin(\phi_S - \phi_H)}$, as a function of the $\pi^{+}$ momentum transverse to the jet axis, $j_{\mathrm{T}}$ with 0.4 < $z$ < 0.8

Collins asymmetries, $A_{\mathrm{UT}}^{\sin(\phi_S - \phi_H)}$, as a function of the $\pi^{-}$ momentum transverse to the jet axis, $j_{\mathrm{T}}$ with 0.4 < $z$ < 0.8

Corrected Yield R=0.5 pi0+jet 15-20 pp at sqrt{s_{NN}}=200 GeV

Corrected Yield R=0.2 gamma+jet 10-15 pp at sqrt{s_{NN}}=200 GeV

Corrected Yield R=0.5 gamma+jet 10-15 pp at sqrt{s_{NN}}=200 GeV

Corrected Yield R=0.5 pi0+jet 10-15 AuAu 0-15% at sqrt{s_{NN}}=200 GeV

Corrected Yield R=0.2 pi0+jet 10-15 AuAu 0-15% at sqrt{s_{NN}}=200 GeV

Corrected Yield R=0.5 pi0+jet 15-20 AuAu 0-15% at sqrt{s_{NN}}=200 GeV

Corrected Yield R=0.2 pi0+jet 15-20 AuAu 0-15% at sqrt{s_{NN}}=200 GeV

Corrected Yield R=0.2 gamma+jet 10-15 AuAu 0-15% at sqrt{s_{NN}}=200 GeV

Corrected Yield R=0.5 gamma+jet 10-15 AuAu 0-15% at sqrt{s_{NN}}=200 GeV

IAA(Δφ) R=0.5 gamma+jet 10-15 GeV/c

IAA(Δφ) R=0.2 gamma+jet 10-15 GeV/c

IAA(Δφ) R=0.5 pi0+jet 10-15 GeV/c

IAA(Δφ) R=0.2 pi0+jet 10-15 GeV/c

IAA(Δφ) R=0.5 pi0+jet 15-20 GeV/c

IAA(Δφ) R=0.2 pi0+jet 15-20 GeV/c

Global polarization of $\Lambda$ and $\bar\Lambda$ and their difference in 20-50\% centrality in Ru+Ru collisions at $\sqrt{s_{NN}}$ = 200 GeV.

Global polarization of $\Lambda$ and $\bar\Lambda$ and their difference in 20-50\% centrality in Zr+Zr collisions at $\sqrt{s_{NN}}$ = 200 GeV.

Global polarization of $\Lambda$ and $\bar\Lambda$ and their difference in 20-50\% centrality in Ru+Ru&Zr+Zr collisions at $\sqrt{s_{NN}}$ = 200 GeV.

Global polarization of $\Lambda$+$\bar\Lambda$ as a function of centrality in the combined Ru+Ru and Zr+Zr collisions at $\sqrt{s_{NN}}$ = 200 GeV (left panel). The data in Au+Au collisions is from Phys. Rev. C 98 (2018) 014910.

Global polarization of $\Lambda$+$\bar\Lambda$ in 20-50\% centrality centrality in the combined Ru+Ru and Zr+Zr collisions at $\sqrt{s_{NN}}$ = 200 GeV (right panel). The data in Au+Au collisions is from Phys. Rev. C 98 (2018) 014910.

Global polarization of $\Lambda$+$\bar\Lambda$ as a function of the average number of participants $\langle N_{\rm part} \rangle$ in the combined Ru+Ru and Zr+Zr collisions at $\sqrt{s_{NN}}$ = 200 GeV. The data in Au+Au collisions is from Phys. Rev. C 98 (2018) 014910.

The transverse momentum dependence of $\Lambda$+$\bar\Lambda$ $P_{\rm H}$ for 20\%-60\% centrality in the combined Ru+Ru and Zr+Zr collisions at $\sqrt{s_{NN}}$ = 200 GeV, together with the results for Au+Au collisions at $\sqrt{s_{NN}}$ = 200 GeV. The data in Au+Au collisions is from Phys. Rev. C 98 (2018) 014910.

The pseudorapidity dependence of $\Lambda$+$\bar\Lambda$ $P_{\rm H}$ for 20\%-60\% centrality in the combined Ru+Ru and Zr+Zr collisions at $\sqrt{s_{NN}}$ = 200 GeV, together with the results for Au+Au collisions at $\sqrt{s_{NN}}$ = 200 GeV. The data in Au+Au collisions is from Phys. Rev. C 98 (2018) 014910.

The polarization coefficient $P_{y,c0}$ of $\Lambda\!+\!\bar\Lambda$ from method-1 and method-2 as a function of centrality (left panel) in isobar Ru+Ru and Zr+Zr collisions at $\sqrt{s_{NN}}$ = 200 GeV. In this figure, $P_{H}$ is same data as in Figure 4.

The polarization coefficient $P_{y,c0}$ of $\Lambda\!+\!\bar\Lambda$ from method-1 and method-2 for 20-50\% centrality (right panel) in isobar Ru+Ru and Zr+Zr collisions at $\sqrt{s_{NN}}$ = 200 GeV. In this figure, $P_{H}$ is same data as in Figure 4.

The polarization coefficient $P_{y,c2}$ of $\Lambda\!+\!\bar\Lambda$ from method-1 and method-2 as a function of centrality (left panel) in isobar Ru+Ru and Zr+Zr collisions at $\sqrt{s_{NN}}$ = 200 GeV.

The polarization coefficient $P_{y,c2}$ of $\Lambda\!+\!\bar\Lambda$ from method-1 and method-2 for 20-50\% centrality (right panel) in isobar Ru+Ru and Zr+Zr collisions at $\sqrt{s_{NN}}$ = 200 GeV.

Global polarization of $\Xi^{-}$+$\bar\Xi^{+}$ from polarization transfer method and direct measurement method as a function of centrality (left panel) in Ru+Ru and Zr+Zr collisions at $\sqrt{s_{NN}}$ = 200 GeV. In this figure, $P_{H}$ of inclusive $\Lambda+\bar\Lambda$ is same data as in Figure 4.

Global polarization of $\Xi^{-}$+$\bar\Xi^{+}$ from polarization transfer method and direct measurement method for 20-50\% centrality (right panel) in Ru+Ru and Zr+Zr collisions at $\sqrt{s_{NN}}$ = 200 GeV . In this figure, $P_{H}$ of inclusive $\Lambda+\bar\Lambda$ is same data as in Figure 4.

The extracted kinetic decoupling temperature is derived from $\pi^{-}$–d correlation functions.

This is the mixed event distribution for $\pi^{+}$–d, required for the fitting

This is the mixed event distribution for $\pi^{-}$–d, required for the fitting

The momentum smearing matrix, required for the fitting, used both for $\pi^{-}$–d and $\pi^{+}$–d

$p_{T}$ dependence of $v_{2}$ for $\pi^{+}$ in Au+Au collisions at 3.9 GeV

$p_{T}$ dependence of $v_{2}$ for $\pi^{+}$ in Au+Au collisions at 4.5 GeV

$p_{T}$ dependence of $v_{2}$ for $\pi^{-}$ in Au+Au collisions at 3 GeV

$p_{T}$ dependence of $v_{2}$ for $\pi^{-}$ in Au+Au collisions at 3.2 GeV

$p_{T}$ dependence of $v_{2}$ for $\pi^{-}$ in Au+Au collisions at 3.5 GeV

$p_{T}$ dependence of $v_{2}$ for $\pi^{-}$ in Au+Au collisions at 3.9 GeV

$p_{T}$ dependence of $v_{2}$ for $\pi^{-}$ in Au+Au collisions at 4.5 GeV

$p_{T}$ dependence of $v_{2}$ for $K^{+}$ in Au+Au collisions at 3 GeV

$p_{T}$ dependence of $v_{2}$ for $K^{+}$ in Au+Au collisions at 3.2 GeV

$p_{T}$ dependence of $v_{2}$ for $K^{+}$ in Au+Au collisions at 3.5 GeV

$p_{T}$ dependence of $v_{2}$ for $K^{+}$ in Au+Au collisions at 3.9 GeV

$p_{T}$ dependence of $v_{2}$ for $K^{+}$ in Au+Au collisions at 4.5 GeV

$p_{T}$ dependence of $v_{2}$ for $K^{-}$ in Au+Au collisions at 3 GeV

$p_{T}$ dependence of $v_{2}$ for $K^{-}$ in Au+Au collisions at 3.2 GeV

$p_{T}$ dependence of $v_{2}$ for $K^{-}$ in Au+Au collisions at 3.5 GeV

$p_{T}$ dependence of $v_{2}$ for $K^{-}$ in Au+Au collisions at 3.9 GeV

$p_{T}$ dependence of $v_{2}$ for $K^{-}$ in Au+Au collisions at 4.5 GeV

$p_{T}$ dependence of $v_{2}$ for $K^{0}_{S}$ in Au+Au collisions at 3 GeV

$p_{T}$ dependence of $v_{2}$ for $K^{0}_{S}$ in Au+Au collisions at 3.2 GeV

$p_{T}$ dependence of $v_{2}$ for $K^{0}_{S}$ in Au+Au collisions at 3.5 GeV

$p_{T}$ dependence of $v_{2}$ for $K^{0}_{S}$ in Au+Au collisions at 3.9 GeV

$p_{T}$ dependence of $v_{2}$ for $K^{0}_{S}$ in Au+Au collisions at 4.5 GeV

$p_{T}$ dependence of $v_{2}$ for $p$ in Au+Au collisions at 3 GeV

$p_{T}$ dependence of $v_{2}$ for $p$ in Au+Au collisions at 3.2 GeV

$p_{T}$ dependence of $v_{2}$ for $p$ in Au+Au collisions at 3.5 GeV

$p_{T}$ dependence of $v_{2}$ for $p$ in Au+Au collisions at 3.9 GeV

$p_{T}$ dependence of $v_{2}$ for $p$ in Au+Au collisions at 4.5 GeV

$p_{T}$ dependence of $v_{2}$ for $\Lambda$ in Au+Au collisions at 3 GeV

$p_{T}$ dependence of $v_{2}$ for $\Lambda$ in Au+Au collisions at 3.2 GeV

$p_{T}$ dependence of $v_{2}$ for $\Lambda$ in Au+Au collisions at 3.5 GeV

$p_{T}$ dependence of $v_{2}$ for $\Lambda$ in Au+Au collisions at 3.9 GeV

$p_{T}$ dependence of $v_{2}$ for $\Lambda$ in Au+Au collisions at 4.5 GeV

The number of constituent quarks $n_q$ scaled $v_2$ as a function of $n_q$ scaled transverse kinetic energy for $\pi^{+}$ at 3 GeV

The number of constituent quarks $n_q$ scaled $v_2$ as a function of $n_q$ scaled transverse kinetic energy for $\pi^{+}$ at 3.2 GeV

The number of constituent quarks $n_q$ scaled $v_2$ as a function of $n_q$ scaled transverse kinetic energy for $\pi^{+}$ at 3.5 GeV

The number of constituent quarks $n_q$ scaled $v_2$ as a function of $n_q$ scaled transverse kinetic energy for $\pi^{+}$ at 3.9 GeV

The number of constituent quarks $n_q$ scaled $v_2$ as a function of $n_q$ scaled transverse kinetic energy for $\pi^{+}$ at 4.5 GeV

The number of constituent quarks $n_q$ scaled $v_2$ as a function of $n_q$ scaled transverse kinetic energy for $\pi^{-}$ at 3 GeV

The number of constituent quarks $n_q$ scaled $v_2$ as a function of $n_q$ scaled transverse kinetic energy for $\pi^{-}$ at 3.2 GeV

The number of constituent quarks $n_q$ scaled $v_2$ as a function of $n_q$ scaled transverse kinetic energy for $\pi^{-}$ at 3.5 GeV

The number of constituent quarks $n_q$ scaled $v_2$ as a function of $n_q$ scaled transverse kinetic energy for $\pi^{-}$ at 3.9 GeV

The number of constituent quarks $n_q$ scaled $v_2$ as a function of $n_q$ scaled transverse kinetic energy for $\pi^{-}$ at 4.5 GeV

The number of constituent quarks $n_q$ scaled $v_2$ as a function of $n_q$ scaled transverse kinetic energy for $K^{+}$ at 3 GeV

The number of constituent quarks $n_q$ scaled $v_2$ as a function of $n_q$ scaled transverse kinetic energy for $K^{+}$ at 3.2 GeV

The number of constituent quarks $n_q$ scaled $v_2$ as a function of $n_q$ scaled transverse kinetic energy for $K^{+}$ at 3.5 GeV

The number of constituent quarks $n_q$ scaled $v_2$ as a function of $n_q$ scaled transverse kinetic energy for $K^{+}$ at 3.9 GeV

The number of constituent quarks $n_q$ scaled $v_2$ as a function of $n_q$ scaled transverse kinetic energy for $K^{+}$ at 4.5 GeV

The number of constituent quarks $n_q$ scaled $v_2$ as a function of $n_q$ scaled transverse kinetic energy for $K^{-}$ at 3 GeV

The number of constituent quarks $n_q$ scaled $v_2$ as a function of $n_q$ scaled transverse kinetic energy for $K^{-}$ at 3.2 GeV

The number of constituent quarks $n_q$ scaled $v_2$ as a function of $n_q$ scaled transverse kinetic energy for $K^{-}$ at 3.5 GeV

The number of constituent quarks $n_q$ scaled $v_2$ as a function of $n_q$ scaled transverse kinetic energy for $K^{-}$ at 3.9 GeV

The number of constituent quarks $n_q$ scaled $v_2$ as a function of $n_q$ scaled transverse kinetic energy for $K^{-}$ at 4.5 GeV

The number of constituent quarks $n_q$ scaled $v_2$ as a function of $n_q$ scaled transverse kinetic energy for $K^{0}_{S}$ at 3 GeV

The number of constituent quarks $n_q$ scaled $v_2$ as a function of $n_q$ scaled transverse kinetic energy for $K^{0}_{S}$ at 3.2 GeV

The number of constituent quarks $n_q$ scaled $v_2$ as a function of $n_q$ scaled transverse kinetic energy for $K^{0}_{S}$ at 3.5 GeV

The number of constituent quarks $n_q$ scaled $v_2$ as a function of $n_q$ scaled transverse kinetic energy for $K^{0}_{S}$ at 3.9 GeV

The number of constituent quarks $n_q$ scaled $v_2$ as a function of $n_q$ scaled transverse kinetic energy for $K^{0}_{S}$ at 4.5 GeV

The number of constituent quarks $n_q$ scaled $v_2$ as a function of $n_q$ scaled transverse kinetic energy for $p$ at 3 GeV

The number of constituent quarks $n_q$ scaled $v_2$ as a function of $n_q$ scaled transverse kinetic energy for $p$ at 3.2 GeV

The number of constituent quarks $n_q$ scaled $v_2$ as a function of $n_q$ scaled transverse kinetic energy for $p$ at 3.5 GeV

The number of constituent quarks $n_q$ scaled $v_2$ as a function of $n_q$ scaled transverse kinetic energy for $p$ at 3.9 GeV

The number of constituent quarks $n_q$ scaled $v_2$ as a function of $n_q$ scaled transverse kinetic energy for $p$ at 4.5 GeV

The number of constituent quarks $n_q$ scaled $v_2$ as a function of $n_q$ scaled transverse kinetic energy for $\Lambda$ at 3 GeV

The number of constituent quarks $n_q$ scaled $v_2$ as a function of $n_q$ scaled transverse kinetic energy for $\Lambda$ at 3.2 GeV

The number of constituent quarks $n_q$ scaled $v_2$ as a function of $n_q$ scaled transverse kinetic energy for $\Lambda$ at 3.5 GeV

The number of constituent quarks $n_q$ scaled $v_2$ as a function of $n_q$ scaled transverse kinetic energy for $\Lambda$ at 3.9 GeV

The number of constituent quarks $n_q$ scaled $v_2$ as a function of $n_q$ scaled transverse kinetic energy for $\Lambda$ at 4.5 GeV

The energy dependence of $p_T$ integrated $v_2$ for $\pi^{\pm}$, $K^{\pm}$, $K^{0}_{S}$, $p$, and $\Lambda$ in 10-40\% centrality from Au+Au collisions at $\sqrt{s_{\text{NN}}}$ = 3.0, 3.2, 3.5, 3.9, and 4.5 GeV.

The energy dependence of $n_{q}$ scaled $v_{2}$ ratios of $v_{2}^{q}(\pi^{+}) / v_{2}^{q}(K^{+})$ and $v_{2}^{q}(p) / v_{2}^{q}(K^{+})$ at ($m_T - m_0$)/$n_q$ = 0.4 GeV/$c^2$

UrQMD model calculations for net-proton cumulant ratios and proton factorial cumulant ratios in Au+Au collisions from $\sqrt{s_{NN}}$ = 7.7 - 200 GeV for 0-5$\%$ centrality. Same choices of centrality definition are used as used for experimental data.

Significance of deviations of central 0-5$\%$ data from various choices of baselines or references.

Cumulant ratios C2/C1 and C4/C2 of net-proton distributions in Au+Au collisions at $\sqrt{s_{NN}}$ = 19.6 GeV as a function of multiplicity (RefMult3X).

Cumulant ratios C2/C1 and C4/C2 of net-proton distributions in Au+Au collisions at $\sqrt{s_{NN}}$ = 19.6 GeV as a function of average multiplicity (RefMult3X) for 8 centrality bins from 0-10$\%$ to 70-80$\%$. Data with and without CBWC are given.

Cumulant ratios C2/C1 and C4/C2 of net-proton distributions in Au+Au collisions at $\sqrt{s_{NN}}$ = 19.6 GeV as a function of average multiplicity (RefMult3X) for 16 centrality bins from 0-5$\%$ to 75-80$\%$. Data with and without CBWC are given.

Reference multiplicity distributions in Au+Au collisions at $\sqrt{s_{NN}}$ = 11.5 GeV from BES-II. Three choices of multiplicity distributions (RefMult3 scaled by efficiency factor of $\epsilon$ = 0.83 or 83$\%$ to mimic RefMult3 of BES-I, RefMult3, and RefMult3X) are presented.

Cumulant ratios C2/C1 and C4/C2 of net-proton distributions in Au+Au collisions at $\sqrt{s_{NN}}$ = 11.5 GeV from BES-II as a function of centrality obtained with various centrality definitions.

Reference multiplicity distributions (RefMult3, RefMult3X, and RefMult3A) in Au+Au collisions at $\sqrt{s_{NN}}$ = 19.6 GeV from UrQMD model. The RefMult3 and RefMult3X distributions have been scaled by an efficiency factor of $\epsilon$ = 77.9$\%$ to mimic the distribution in experimenal data.

Cumulant ratios C2/C1 and C4/C2 of net-proton distributions in Au+Au collisions at $\sqrt{s_{NN}}$ = 19.6 GeV from UrQMD model as a function of centrality obtained with various centrality definitions (RefMult3, RefMult3X, and RefMult3A). The RefMult3 and RefMult3X distributions have been scaled by an efficiency factor of $\epsilon$ = 77.9$\%$ to mimic the distribution in experimenal data.

Collision energy dependence of net-proton C4/C2 in Au+Au collisions at $\sqrt{s_{NN}}$ = 7.7 - 27 GeV from BES-II obtained with RefMult3 centrality definition.

Difference between net-proton C4/C2 (0-5$\%$) data from various choices of baselines or references as a function of collision energy from $\sqrt{s_{NN}}$ = 7.7 - 200 GeV.