arXiv subjects

G. Chen

Publications and source records attributed to G. Chen.

At least 685 records · Page 38Linked to original sources

arXiv2020

Measurement of the cross section for $e^{+}e^{-}\rightarrowΞ^{-}\barΞ^{+}$ and observation of an excited $Ξ$ baryon

Using a total of 11.0 fb$^{-1}$ of $e^{+}e^{-}$ collision data with center-of-mass energies between 4.009 GeV and 4.6 GeV and collected with the BESIII detector at BEPCII, we measure fifteen exclusive cross sections and effective form factors for the process $e^{+}e^{-}\rightarrowΞ^{-}\barΞ^{+}$ by means of a single baryon-tag method. After performing a fit to the dressed cross section of $e^{+}e^{-}\rightarrowΞ^{-}\barΞ^{+}$, no significant $ψ(4230)$ or $ψ(4260)$ resonance is observed in the $Ξ^{-}\barΞ^{+}$ final states, and upper limits at the 90\% confidence level on $Γ_{ee}\mathcal{B}$ for the processes $ψ(4230)$/$ψ(4260)\rightarrowΞ^{-}\barΞ^{+}$ are determined. In addition, an excited $Ξ$ baryon at 1820 MeV/$c^{2}$ is observed with a statistical significance of 6.2 $\sim$ 6.5$σ$ by including the systematic uncertainty, and the mass and width are measured to be $M = (1825.5 \pm 4.7 \pm 4.7)$~MeV/$c^{2}$ and $Γ= (17.0 \pm 15.0 \pm 7.9)$~MeV, which confirms the existence of the $J^{P}=\frac{3}{2}^{-}$ state $Ξ(1820)$.

hep-ex↗

arXiv2020

Joint Analysis of Energy and RMS Spectra from MAXI J1535-571 with Insight-HXMT

A new black hole X-ray binary (BHXRB) MAXI J1535-571 was discovered by MAXI during its outburst in 2017. Using observations taken by the first Chinese X-ray satellite, the Hard X-ray Modulation Telescope (dubbed as Insight-HXMT), we perform a joint spectral analysis (2-150 keV) in both energy and time domains. The energy spectra provide the essential input for probing the intrinsic Quasi-Periodic Oscillation (QPO) fractional rms spectra (FRS). Our results show that during the intermediate state, the energy spectra are in general consistent with those reported by Swift/XRT and NuSTAR. However, the QPO FRS become harder and the FRS residuals may suggest the presence of either an additional power-law component in the energy spectrum or a turn-over in the intrinsic QPO FRS at high energies.

astro-ph.HE↗

arXiv2020

Cross section measurement of $e^+e^- \rightarrow η'J/ψ$ from $\sqrt{s} = 4.178$ to $4.600$ GeV

The cross section of the process $e^+e^- \rightarrow η'J/ψ$ is measured at center-of-mass energies from $\sqrt{s} =$ 4.178 to 4.600 GeV using data samples corresponding to a total integrated luminosity of 11 fb$^{-1}$ collected with the BESIII detector operating at the BEPCII storage ring. The dependence of the cross section on $\sqrt{s}$ shows an enhancement around $4.2$ GeV. While the shape of the cross section cannot be fully explained with a single $ψ(4160)$ or $ψ(4260)$ state, a coherent sum of the two states does provide a reasonable description of the data.

hep-ex↗

arXiv2020

Observation of a resonant structure in $e^{+}e^{-} \to K^{+}K^{-}π^{0}π^{0}$

Using $e^{+}e^{-}$ collision data samples with center-of-mass energies ranging from 2.000 to 2.644 GeV, collected by the BESIII detector at the BEPCII collider, and with a total integrated luminosity of 300 pb^{-1}, a partial-wave analysis is performed for the process $e^{+}e^{-} \to K^{+}K^{-}π^{0}π^{0}$. The total Born cross sections for the process $e^{+}e^{-} \to K^{+}K^{-}π^{0}π^{0}$, as well as the Born cross sections f or the subprocesses $e^{+}e^{-} \to ϕπ^{0}π^{0}$, $K^{+}(1460)K^{-}$, $K^{+}_{1}(1400)K^{-}$, $K^{+}_{1}(1270)K^{-}$ and $K^{*+}(892)K^{*-}(892)$, are measured versus the center-of-mass energy. The corresponding results for $e^{+}e^{-} \to K^{+}K^{-}π^{0}π^{0}$ and $ϕπ^{0}π^{0}$ are consistent with those of BaBar and have much improved precision.By analyzing the cross sections for the four subprocesses, $K^{+}(1460)K^{-}$, $K^{+}_{1}(1400)K^{-}$, $K^{+ }_{1}(1270)K^{-}$ and $K^{*+}K^{*-}$, a structure with mass $M$ = (2126.5 $\pm$ 16.8 $\pm$ 12.4)~MeV/c^{2} and width $Γ$ = (106.9 $\pm$ 32.1 $\pm$ 28.1)~MeV is observed with an overall statistical significance of 6.3 $σ$, although with very limited significance in the subprocesses $e^{+}e^{-} \to K^{+}_{1}(1270)K^{-}$ and $K^{*+}(892)K^{*-}(892)$. The resonant parameters of the observed structure suggest it can be identified with the $ϕ(2170)$, thus the results provide valuable input to the internal nature of the $ϕ(2170)$.

hep-ex↗

arXiv2020

Measurement of {\boldmath $J/ψ\toΞ(1530)^{-}\barΞ^{+}$} and evidence for the radiative decay {\boldmath $Ξ(1530)^{-}\toγΞ^-$}

The SU(3)-flavor violating decay $J/ψ\toΞ(1530)^{-}\barΞ^{+}+c.c.$ is studied using $(1310.6\pm7.0)\times 10^{6} ~J/ψ$ events collected with the BESIII detector at BEPCII and the branching fraction is measured to be ${\cal{B}}(J/ψ\toΞ(1530)^{-}\barΞ^{+}+c.c.)=(3.17\pm0.02_{\rm stat.}\pm0.08_{\rm syst.})\times10^{-4}$. This is consistent with previous measurements with an improved precision. The angular parameter for this decay is measured for the first time and is found to be $α=-0.21\pm0.04_{\rm stat.}\pm0.06_{\rm syst.}$. In addition, we report evidence for the radiative decay $Ξ(1530)^{-}\toγΞ^- $ with a significance of 3.9$σ$, including the systematic uncertainties. The 90\% confidence level upper limit on the branching fraction is determined to be $\mathcal{B}(Ξ(1530)^{-}\toγΞ^- )\leq3.7$\%.

hep-ex↗

arXiv2019

Measurement of the $e^+e^-\toπ^+π^-π^0$ cross section from 0.7 GeV to 3.0 GeV via initial-state radiation

The cross section of the process $e^+e^-\toπ^+π^-π^0$ is measured with a precision of 1.6% to 25% in the energy range between $0.7$ and 3.0 GeV using the Initial State Radiation method. A data set with an integrated luminosity of $2.93$fb$^{-1}$ taken at the center-of-mass energy of $\sqrt{s}=3.773$GeV with the BESIII detector at the BEPCII collider is used. The product branching fractions for $ω$, $ϕ$, $ω(1420)$, and $ω(1650)$ are measured to be $\mathcal{B}(ω\to e^+e^-) \times \mathcal{B}(ω\to π^+π^-π^0)=(6.94\pm0.08\pm0.16) \times 10^{-5}$, $\mathcal{B}(ϕ\to e^+e^-) \times \mathcal{B}(ϕ\toπ^+π^-π^0) = (4.20\pm0.08\pm0.19) \times 10^{-5}$, $\mathcal{B}(ω(1420)\to e^+e^-) \times \mathcal{B}(ω(1420) \to π^+π^-π^0) = (0.84\pm0.09\pm0.09) \times 10^{-6}$, and $\mathcal{B}(ω(1650) \to e^+e^) \times \mathcal{B}(ω(1650)\to π^+π^-π^0) = (1.14\pm0.15\pm0.15)\times10^{-6}$, respectively. The branching fraction $\mathcal{B}(J/ψ\to π^+π^-π^0)$ is measured to be $(2.188 \pm 0.024 \pm 0.024 \pm0.040 (Γ_{ee}^{J/ψ}))\%$, where $Γ_{ee}^{J/ψ}$ is the dileptonic width of $J/ψ$. The first errors are of statistical, the second and third ones of systematic nature.

hep-ex↗

arXiv2019

Observation of the $X(2370)$ and search for the $X(2120)$ in $J/ψ\toγK\bar{K} η'$

Using a sample of $1.31\times10^{9} ~J/ψ$ events collected with the BESIII detector, we perform a study of $J/ψ\toγK\bar{K}η'$. The $X(2370)$ is observed in the $K\bar{K}η'$ invariant-mass distribution with a statistical significance of 8.3$σ$. Its resonance parameters are measured to be $M = 2341.6 \pm 6.5\text{(stat.)} \pm 5.7\text{(syst.)}$~MeV/$c^{2}$ and $Γ= 117 \pm 10 \text{(stat.)} \pm 8 \text{(syst.)}$~MeV. The product branching fractions for $J/ψ\to γX(2370), X(2370) \to K^{+} K^{-}η'$ and $J/ψ\to γX(2370), X(2370) \to K_{S}^{0} K_{S}^{0}η'$ are determined to be $(1.79 \pm 0.23 \text{(stat.)} \pm 0.65 \text{(syst.)}) \times 10^{-5}$ and $(1.18 \pm 0.32\ text{(stat.)} \pm 0.39 \text{(syst.)}) \times 10^{-5}$, respectively. No evident signal for the $X(2120)$ is observed in the $K\bar{K}η'$ invariant-mass distribution. The upper limits for the product branching fractions of $\mathcal{B}(J/ψ\to γX(2120)\toγK^{+} K^{-} η')$ and $\mathcal{B}(J/ψ\toγX(2120)\toγK_{S}^{0} K_{S}^{0} η')$ are determined to be $1.49\times10^{-5}$ and $6.38\times10^{-6}$ at the 90% confidence level, respectively.

hep-ex↗

arXiv2019

Diagnostic of the spectral properties of Aquila X-1 by Insight-HXMT snapshots during the early propeller phase

We study the 2018 outburst of Aql X-1 via the monitor of all sky X-ray image (MAXI) data. We show that the outburst starting in February 2018 is a member of short-low class in the frame of outburst duration and the peak count rate although the outburst morphology is slightly different from the other fast-rise-exponential-decay (FRED) type outbursts with a milder rising stage. We study the partial accretion in the weak propeller stage of Aql X-1 via the MAXI data of the 2018 outburst. We report on the spectral analysis of 3 observations of Aquila X-1 obtained by Insight - hard X-ray modulation telescope (Insight-HXMT) during the late decay stage of the 2018 outburst. We discuss that the data taken by Insight-HXMT is just after the transition to the weak propeller stage. Our analysis shows the necessity of a comptonization component to take into account the existence of an electron cloud resulting photons partly up-scattered.

astro-ph.HE↗

arXiv2019

Observation of the Semileptonic $D^+$ Transition into an Axial-Vector Meson $\bar K_1(1270)^0$

By analyzing a 2.93~$\rm fb^{-1}$ data sample of $e^+e^-$ collisions, recorded at a center-of-mass energy of 3.773 $\rm \,GeV$ with the BESIII detector operated at the BEPCII collider, we have searched for the semileptonic $D^+$ transition into the axial-vector meson ${\bar{K}}_{1}(1270)^{0}$. The $D^{+} \rightarrow {\bar{K}}_{1}(1270)^{0}e^{+}ν_{e}$ decay is observed for the first time with a statistical significance greater than $10σ$. Its decay branching fraction is determined to be ${\mathcal B}[D^+\to \bar K_1(1270)^0 e^+ν_e]=(2.30\pm0.26\pm 0.18 \pm 0.25)\times10^{-3}$, where the first and second uncertainties are statistical and systematic, respectively, and the third originates from the input branching fraction of ${\bar{K}}_{1}(1270)^{0} \rightarrow K^{-} π^{+} π^{0}$.

hep-ex↗

arXiv2019

Measurement of Branching Fractions of $ψ(3686)\rightarrowϕη^\prime, ϕf_1(1285)$ and $ϕη(1405)$

Using a sample of $448.1\times10^6$ $ψ(3686)$ events collected with the BESIII detector, we perform a study of the decay $ψ(3686) \rightarrow ϕπ^{+}π^{-}η$. The branching fraction of $ψ(3686)\rightarrowϕη^\prime$ is determined to be $(1.51\pm0.16\pm0.12)\times 10^{-5}$, which is consistent with the previous measurement but with significantly improved precision. The resonances $f_{1}(1285)$ and $η(1405)$ are clearly observed in the $π^{+}π^{-}η$ mass spectrum with statistical significances of $18σ$ and $9.7σ$, respectively. The corresponding product branching fractions are measured to be $\mathcal{B}(ψ(3686)\rightarrowϕf_{1}(1285),f_{1}(1285)\rightarrowπ^{+}π^{-}η) =(1.03\pm0.10\pm0.09)\times 10^{-5}$ and $\mathcal{B}(ψ(3686)\rightarrowϕη(1405),η(1405)\rightarrowπ^{+}π^{-}η) =(8.46\pm1.37\pm0.92)\times 10^{-6}$.

hep-ex↗

arXiv2019

Observation of the leptonic decay $D^+ \to τ^+ ν_τ$

We report the first observation of $D^+\toτ^+ν_τ$ with a significance of $5.1σ$. We measure ${\cal B}(D^+\toτ^+ν_τ) = (1.20\pm0.24_{\text{stat.}}\pm0.12_{\text{syst.}})\times10^{-3}$. Taking the world average ${\cal B}(D^+\toμ^+ν_μ) = (3.74\pm0.17)\times10^{-4}$, we obtain $R_{τ/μ} =Γ(D^+\toτ^+ν_τ)/Γ(D^+\toμ^+ν_μ) = 3.21\pm0.64_{\text{stat.}}\pm0.43_{\text{syst.}}$, which is consistent with the Standard Model expectation of lepton flavor universality. Using external inputs, our results give values for the $D^+$ decay constant $f_{D^+}$ and the CKM matrix element $|V_{cd}|$ that are consistent with, but less precise than, other determinations.

hep-ex↗

arXiv2019

Partial-wave analysis of $J/ψ\to K^+K^-π^0$

A partial-wave analysis of the decay $J/ψ\to K^+K^-π^0$ has been made using $(223.7\pm1.4)\times 10^{6}$ $J/ψ$ events collected with the BESIII detector in 2009. The analysis, which is performed within the isobar-model approach, reveals contributions from $K^*_2(1430)^\pm$, $K^*_2(1980)^\pm$ and $K^*_4(2045)^\pm$ decaying to $K^\pmπ^0$. The two latter states are observed in $J/ψ$ decays for the first time. Two resonance signals decaying to $K^+K^-$ are also observed. These contributions can not be reliably identified and their possible interpretations are discussed. The measured branching fraction $B(J/ψ\to K^+K^-π^0)$ of $(2.88\pm0.01\pm0.12)\times10^{-3}$ is more precise than previous results. Branching fractions for the reported contributions are presented as well. The results of the partial-wave analysis differ significantly from those previously obtained by BESII and BABAR.

hep-ex↗

arXiv2019

Observation of the decays $χ_{cJ} \to ϕϕη$

Using a data sample of $(448.1\pm2.9)\times10^{6}$ $ψ(3686)$ decays collected by the BESIII detector at the Beijing Electron Positron Collider (BEPCII), we observe the decays $χ_{cJ}\to ϕϕη~(J=0,~1,~2)$, where the $χ_{cJ}$ are produced via the radiative processes $ψ(3686)\toγχ_{cJ}$. The branching fractions are measured to be $\mathcal B(χ_{c0}\toϕϕη)=(8.41\pm0.74\pm0.62)\times10^{-4}$, $\mathcal B(χ_{c1}\toϕϕη)=(2.96\pm0.43\pm0.22)\times 10^{-4}$, and $\mathcal B(χ_{c2} \to ϕϕη)=(5.33\pm0.52\pm0.39) \times 10^{-4}$, where the first uncertainties are statistical and the second are systematic. We also search for intermediate states in the $ϕϕ$ or $ηϕ$ combinations, but no significant structure is seen due to the limited statistics.

hep-ex↗

arXiv2019

Ionized calcium in the atmospheres of two ultra-hot exoplanets WASP-33b and KELT-9b

Ultra-hot Jupiters are emerging as a new class of exoplanets. Studying their chemical compositions and temperature structures will improve the understanding of their mass loss rate as well as their formation and evolution. We present the detection of ionized calcium in the two hottest giant exoplanets - KELT-9b and WASP-33b. By utilizing transit datasets from CARMENES and HARPS-N observations, we achieved high confidence level detections of Ca II using the cross-correlation method. We further obtain the transmission spectra around the individual lines of the Ca II H&K doublet and the near-infrared triplet, and measure their line profiles. The Ca II H&K lines have an average line depth of 2.02 $\pm$ 0.17 % (effective radius of 1.56 Rp) for WASP-33b and an average line depth of 0.78 $\pm$ 0.04 % (effective radius of 1.47 Rp) for KELT-9b, which indicates that the absorptions are from very high upper atmosphere layers close to the planetary Roche lobes. The observed Ca II lines are significantly deeper than the predicted values from the hydrostatic models. Such a discrepancy is probably a result of hydrodynamic outflow that transports a significant amount of Ca II into the upper atmosphere. The prominent Ca II detection with the lack of significant Ca I detection implies that calcium is mostly ionized in the upper atmospheres of the two planets.

astro-ph.EP↗

arXiv2019

Kojima-1Lb Is a Mildly Cold Neptune around the Brightest Microlensing Host Star

We report the analysis of additional multiband photometry and spectroscopy and new adaptive optics (AO) imaging of the nearby planetary microlensing event TCP J05074264+2447555 (Kojima-1), which was discovered toward the Galactic anticenter in 2017 (Nucita et al.). We confirm the planetary nature of the light-curve anomaly around the peak while finding no additional planetary feature in this event. We also confirm the presence of apparent blending flux and the absence of significant parallax signal reported in the literature. The AO image reveals no contaminating sources, making it most likely that the blending flux comes from the lens star. The measured multiband lens flux, combined with a constraint from the microlensing model, allows us to narrow down the previously unresolved mass and distance of the lens system. We find that the primary lens is a dwarf on the K/M boundary (0.581 \pm 0.033 M_sun) located at 505 \pm 47 pc and the companion (Kojima-1Lb) is a Neptune-mass planet (20.0 \pm 2.0 M_earth) with a semi-major axis of 1.08 ^{+0.62}_{-0.18} au. This orbit is a few times smaller than those of typical microlensing planets and is comparable to the snow-line location at young ages. We calculate that the a priori detection probability of Kojima-1Lb is only \sim 35%, which may imply that Neptunes are common around the snow line, as recently suggested by the transit and radial velocity techniques. The host star is the brightest among the microlensing planetary systems (Ks = 13.7), offering a great opportunity to spectroscopically characterize this system, even with current facilities.

astro-ph.EP↗

arXiv2019

Search for the decay $D_{s}^{+} \to p\bar{p}e^{+}ν_{e}$

Using a $3.19~\mathrm{fb}^{-1}$ data sample collected at the $\sqrt{s}~=~4.178$ GeV with the BESIII detector, we search for the rare decay $D_{s}^{+} \rightarrow p \bar{p} e^{+} ν_{e} $. No significant signal is observed, and an upper limit of $\mathcal{B}(D_{s}^{+} \rightarrow p \bar{p} e^{+} ν_{e}) < 2.0 \times 10^{-4}$ is set at the 90\% confidence level. This measurement is useful input in understanding the baryonic transition of $D_{s}^{+}$ mesons.

hep-ex↗

arXiv2019

Insight-HXMT observation on 4U~1608--52: evolving spectral properties of a bright type-I X-ray burst

The evidences for the influence of thermonuclear (type-I) X-ray bursts upon the surrounding environments in neutron star low-mass X-ray binaries (LMXB) were detected previously via spectral and timing analyses. Benefitting from a broad energy coverage of Insight-HXMT, we analyze one photospheric radius expansion (PRE) burst, and find an emission excess at soft X-rays. Our spectral analysis shows that, such an excess is not likely relevant to the disk reflection induced by the burst emission and can be attributed to an enhanced pre-burst/persistent emission. We find that the burst and enhanced persistent emissions sum up to exceed Eddington luminosity by $\sim$ 40 percentages. We speculate that the enhanced emission is from a region beyond the PRE radius, or through the Comptonization of the corona.

astro-ph.HE↗

arXiv2019

$Insight$-HXMT study of the timing properties of Sco X-1

We present a detailed timing study of the brightest persistent X-ray source Sco X-1 using the data collected by the Hard X-ray Modulation Telescope ($Insight$-HXMT) from July 2017 to August 2018. A complete $Z$-track hardness-intensity diagram (HID) is obtained. The normal branch oscillations (NBOs) at $\sim$ 6 Hz in the lower part of the normal branch (NB) and the flare branch oscillations (FBOs) at $\sim$ 16 Hz in the beginning part of the flaring branch (FB) are found in observations with the Low Energy X-ray Telescope (LE) and the Medium Energy X-ray Telescope (ME) of $Insight$-HXMT, while the horizontal branch oscillations (HBOs) at $\sim$ 40 Hz and the kilohertz quasi-periodic oscillations (kHz QPOs) at $\sim$ 800 Hz are found simultaneously up to 60 keV for the first time on the horizontal branch (HB) by the High Energy X-ray Telescope (HE) and ME. We find that for all types of the observed QPOs, the centroid frequencies are independent of energy, while the root mean square (rms) increases with energy; the centroid frequencies of both the HBOs and kHz QPOs increase along the $Z$-track from the top to the bottom of the HB; and the NBOs show soft phase lags increasing with energy. A continuous QPO transition from the FB to NB in $\sim$ 200 s are also detected. Our results indicate that the non-thermal emission is the origin of all types of QPOs, the innermost region of the accretion disk is non-thermal in nature, and the corona is nonhomogeneous geometrically.

astro-ph.HE↗