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1. ATOMS: ALMA Three-millimeter Observations of massive Star-forming regions -XX. Probability distribution function of integrated intensity for dense molecular gas tracers

Author: Zhang, C., Liu, Tie, Jiao, Sihan, Zhu, Feng-Yao, Ren, Z. -Y., Liu, H. -L., Wang, Ke, Wu, J. -W., Li, D., García, P., Garay, Guido, Bronfman, Leonardo, Juvela, Mika, das, Swagat, Lee, Chang Won, Xu, Feng-Wei, Tóth, L. V., Gorai, Prasanta, and Sanhueza, Patricio
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We report the observations of J=1-0 of HCN, HCO+, H13CO+, and H13CN, HC3N (J=11-10) emission towards 135 massive star-forming clumps, as part of the ATOMS (ALMA Three-millimeter Observations of Massive Star-forming regions) Survey. We present the integrated intensity probability distribution function for these molecular tracers, modeled as a combination of a log-normal distribution and a power-law tail. The molecular line luminosities for the power-law tail segment, Lmol(p), have been calculated. We have investigated the correlation between the bolometric luminosity, Lbol, and the power-law part of the molecular line luminosity, Lmol(p). Our findings suggest that the scaling relationships between Lbol and Lmol(p) for HCN and HCO+ are sublinear, indicating that these molecules might not be the most effective tracers for the dense gas. In contrast, H13CN and HC3N exhibit a nearly linear relationship between Lbol and Lmol(p), indicating that they can well trace gravitationally bound dense gas. The ratios of Lbol-to-Lmol(p), serving as indicators of star formation efficiency within massive star-forming clumps, exhibit a weak anti-correlation with the power-law index in the I-PDF. In addition, the star formation efficiency is also weakly anti-correlated with the exponent U of the corresponding equivalent density distribution. Our results implie that clumps with substantial gas accumulation may still display low star formation efficiencies.
Published: 2025

2. ALMA-IMF XVI: Mass-averaged temperature of cores and protostellar luminosities in the ALMA-IMF protoclusters

Author: Motte, F., Pouteau, Y., Nony, T., Dell'Ova, P., Gusdorf, A., Brouillet, N., Stutz, A. M., Bontemps, S., Ginsburg, A., Csengeri, T., Men'shchikov, A., Valeille-Manet, M., Louvet, F., Bonfand, M., Galván-Madrid, R., Álvarez-Gutiérrez, R. H., Armante, M., Bronfman, L., Chen, H. -R. V., Cunningham, N., Díaz-González, D., Didelon, P., Fernández-López, M., Herpin, F., Kessler, N., Koley, A., Lefloch, B., Nestour, N. Le, Liu, H. -L., Moraux, E., Luong, Q. Nguyen, Olguin, F., Salinas, J., Sandoval-Garrido, N. A., Sanhueza, P., Veyry, R., and Yoo, T.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: ALMA-IMF imaged 15 massive protoclusters down to a resolution of of 2 kau scales, identifying about 1000 star-forming cores. The mass and luminosity of these cores, which are fundamental physical characteristics, are difficult to determine, a problem greatly exacerbated at the distances >2 kpc of ALMA-IMF protoclusters. We combined new datasets and radiative transfer modeling to characterize these cores. We estimated their mass-averaged temperature and the masses these estimates imply. For 1/6 of the sample, we measured the bolometric luminosities, implementing deblending corrections when necessary. We used spectral energy distribution (SED) analysis obtained with the PPMAP Bayesian procedure, which aims to preserve the best angular resolution of the input data. We extrapolated the luminosity and dust temperature images provided by PPMAP at 2.5" resolution to estimate those of individual cores, which were identified at higher angular resolution. To do this, we applied approximate radiative transfer relationships between the luminosity of a protostar and the temperature of its surrounding envelope and between the external heating of prestellar cores and their temperatures. For the first time, we provide data-informed estimates of dust temperatures for 883 cores identified with ALMA-IMF: 17-31 K and 28-79 K (5th and 95th percentiles, up to 127 K) for the 617 prestellar and 266 protostellar cores, respectively. We also measured protostellar luminosities spanning 20-80 000 Lsun. For hot cores, we estimated systematically lower temperatures than studies based on complex organic molecules. We established a mass-luminosity evolutionary diagram, for the first time at the core spatial resolution and for a large sample of high-mass protostellar cores. The ALMA-IMF data favor a scenario in which protostars accrete their mass from a larger mass reservoir than their host cores., Comment: 42 pages, 13 figures, accepted by A&A
Published: 2024
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3. ALMA-IMF XVIII: The assembly of a star cluster: Dense N$_2$H$^+$ (1-0) kinematics in the massive G351.77 protocluster

Author: Sandoval-Garrido, N. A., Stutz, A. M., Álvarez-Gutiérrez, R. H., Galván-Madrid, R., Motte, F., Ginsburg, A., Cunningham, N., Reyes-Reyes, S., Redaelli, E., Bonfand, M., Salinas, J., Koley, A., Braine, J., Bronfman, L., Busquet, G., Csengeri, T., Di Francesco, J., Fernández-López, M., Garcia, P., Gusdorf, A., Liu, H. -L., and Sanhueza, P.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: ALMA-IMF observed 15 massive protoclusters capturing multiple spectral lines and the continuum emission. We focus on the G351.77 protocluster ($\sim$ 2500 M$_{\odot}$, estimated from single-dish continuum observations) located at 2 kpc. We trace the dense gas emission and kinematics with N$_2$H$^+$ (1-0) at $\sim$ 4 kau resolution. We estimate an N$_2$H$^+$ relative abundance $\sim (1.7 \pm 0.5) \times 10^{-10}$. We decompose the N$_2$H$^+$ emission into up to two velocity components, highlighting the kinematic complexity in the dense gas. By examining the position-velocity (PV) diagrams on small scales, we observe clear inflow signatures (V-shapes) associated with dense cores. The most prominent V-shape has a mass inflow rate of $\sim 9.8 \times 10^{-4}$ M$_{\odot}$ yr$^{-1}$ and a short timescale of $\sim$ 15.6 kyr. We also observe V-shapes without associated cores. This suggests both that cores or centers of accretion exist below the 1.3 mm detection limit, and that the V-shapes may be viable tracers of very early accretion and star formation on $\sim$ 4 kau scales. The large-scale PV diagram shows that the protocluster is separated into 2 principal velocity structures. Combined with smaller scale DCN and H$_2$CO emission, we propose a scenario of larger scale slow contraction with rotation in the center based on simple toy models. This scenario leads the suggestion of outside-in evolution of the protocluster as it collapses. The gas depletion times implied by the V-shapes are short ($\sim$ 0.3 Myr), requiring either very fast cluster formation, and/or continuous mass feeding of the protocluster. The latter is possible via the Mother Filament G351.77 is forming out of. The similarities in the properties of G351.77 and the recently published work in G353.41 indicate that many of the physical conditions inferred via the ALMA-IMF N$_2$H$^+$ observations may be generic to protoclusters., Comment: Submitted in A&A, 28 pages, 31 figures, 4 interactive figures, 7 tables
Published: 2024

4. ALMA-IMF XV: The core mass function in the high-mass star-formation regime

Author: Louvet, F., Sanhueza, P., Stutz, A., Men'shchikov, A., Motte, F., Galván-Madrid, R., Bontemps, S., Pouteau, Y., Ginsburg, A., Csengeri, T., Di Francesco, J., Dell'Ova, P., González, M., Didelon, P., Braine, J., Cunningham, N., Thomasson, B., Lesaffre, P., Hennebelle, P., Bonfand, M., Gusdorf, A., Álverez-Gutiérrez, R. H., Nony, T., Busquet, G., Olguin, F., Bronfman, L., Salinas, J., Fernandez-Lopez, M., Moraux, E., Liu, H. L., Lu, X., Huei-Ru, V., Towner, A., Valeille-Manet, M., Brouillet, N., Herpin, F., Lefloch, B., Baug, T., Maud, L., Lopez-Sepulcre, A., and Svodoba, B.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: The stellar initial mass function (IMF) is critical to our understanding of star formation and the effects of young stars on their environment. On large scales, it enables us to use tracers such as UV or Halpha emission to estimate the star formation rate of a system and interpret unresolved star clusters across the universe. So far, there is little firm evidence of large-scale variations of the IMF, which is thus generally considered universal. Stars form from cores and it is now possible to estimate core masses and compare the core mass function (CMF) with the IMF, which it presumably produces. The goal of the ALMA-IMF large program is to measure the core mass function at high linear resolution (2700 au) in 15 typical Milky Way protoclusters spanning a mass range of 2500 to 32700 Msun. In this work, we used two different core extraction algorithms to extract about 680 gravitationally bound cores from these 15 protoclusters. We adopt per core temperature using the temperature estimate from the PPMAP Bayesian method. A power-law fit to the CMF of the sub-sample of cores above the 1.64 Msun completeness limit, 330 cores, through the maximum likelihood estimate technique yields a slope of 1.97 +/- 0.06, significantly flatter than the 2.35 Salpeter slope. Assuming a self-similar mapping between the CMF and the IMF, this result implies that these 15 high-mass protoclusters will generate atypical IMFs. This sample is the largest to date produced and analysed self-consistently, derived at matched physical resolution, with per-core temperature estimates and cores as massive as 150 Msun. We provide the raw source extraction catalogues and the source derived size, temperature, mass, and spectral indices in the 15 protoclusters., Comment: Accepted by A&A
Published: 2024
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5. ALMA-IMF XII: Point-process mapping of 15 massive protoclusters

Author: Dell'Ova, P., Motte, F., Gusdorf, A., Pouteau, Y., Men'shchikov, A., Diaz-Gonzalez, D., Galván-Madrid, R., Lesaffre, P., Didelon, P., Stutz, A. M., Towner, A. P. M., Marsh, K., Whitworth, A., Armante, M., Bonfand, M., Nony, T., Valeille-Manet, M., Bontemps, S., Csengeri, T., Cunningham, N., Ginsburg, A., Louvet, F., Alvarez-Gutierrez, R. H., Brouillet, N., Salinas, J., Sanhueza, P., Nakamura, F., Luong, Q. Nguyen, Baug, T., Fernandez-Lopez, M., Liu, H. -L., and Olguin, F.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: A crucial aspect in addressing the challenge of measuring the core mass function, that is pivotal for comprehending the origin of the initial mass function, lies in constraining the temperatures of the cores. We aim to measure the luminosity, mass, column density and dust temperature of star-forming regions imaged by the ALMA-IMF large program. High angular resolution mapping is required to capture the properties of protostellar and pre-stellar cores and to effectively separate them from larger features, such as dusty filaments. We employed the point process mapping (PPMAP) technique, enabling us to perform spectral energy distribution fitting of far-infrared and submillimeter observations across the 15 ALMA-IMF fields, at an unmatched 2.5" angular resolution. By combining the modified blackbody model with near-infrared data, we derived bolometric luminosity maps. We estimated the errors impacting values of each pixel in the temperature, column density, and luminosity maps. Subsequently, we employed the extraction algorithm getsf on the luminosity maps in order to detect luminosity peaks and measure their associated masses. We obtained high-resolution constraints on the luminosity, dust temperature, and mass of protoclusters, that are in agreement with previously reported measurements made at a coarser angular resolution. We find that the luminosity-to-mass ratio correlates with the evolutionary stage of the studied regions, albeit with intra-region variability. We compiled a PPMAP source catalog of 313 luminosity peaks using getsf on the derived bolometric luminosity maps. The PPMAP source catalog provides constraints on the mass and luminosity of protostars and cores, although one source may encompass several objects. Finally, we compare the estimated luminosity-to-mass ratio of PPMAP sources with evolutionary tracks and discuss the limitations imposed by the 2.5" beam., Comment: 35 pages, 19 figures, 5 tables Accepted by A&A
Published: 2024

6. On p-radical covers of pentavalent arc-transitive graphs

Author: Liu, H. L. and Ma, Y. L.
Published: 2024
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7. ALMA-IMF XIII: N$_2$H$^+$ kinematic analysis on the intermediate protocluster G353.41

Author: Álvarez-Gutiérrez, R. H., Stutz, A. M., Sandoval-Garrido, N., Louvet, F., Motte, F., Galván-Madrid, R., Cunningham, N., Sanhueza, P., Bonfand, M., Bontemps, S., Gusdorf, A., Ginsburg, A., Csengeri, T., Reyes, S. D., Salinas, J., Baug, T., Bronfman, L., Busquet, G., Díaz-González, D. J., Fernandez-Lopez, M., Guzmán, A., Koley, A., Liu, H. -L., Olguin, F. A., Valeille-Manet, M., and Wyrowski, F.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: The ALMA-IMF Large Program provides multi-tracer observations of 15 Galactic massive protoclusters at matched sensitivity and spatial resolution. We focus on the dense gas kinematics of the G353.41 protocluster traced by N$_2$H$^+$ (1$-$0), with an spatial resolution $\sim$0.02 pc. G353.41, at a distance of $\sim$2 kpc, has a mass of $\sim$2500 M$_{\odot}$ within $1.3\times1.3$ pc$^2$. We extract the N$_2$H$^+$ isolated line component and we decompose it by fitting up to 3 Gaussian velocity components. This allows us to identify velocity structures that are impossible to identify in the traditional position-velocity diagram. We identify multiple velocity gradients on large ($\sim$1 pc) and small scales ($\sim$0.2 pc). We find good agreement between the N$_2$H$^+$ velocities and the previously reported DCN core velocities, suggesting that cores are kinematically coupled to the dense gas in which they form. We measure 9 converging ``V-shaped'' velocity gradients ($\sim20$ km/s/pc), located in filaments, which are sometimes associated with cores near their point of convergence. The average inflow timescale is $\sim67$ kyr, or about twice the free-fall time of cores in the same area ($\sim33$ kyr) but substantially shorter than protostar lifetime estimates ($\sim$0.5 Myr). We derive mass accretion rates in the range of $(0.35-8.77)\,\times\,10^{-4}$ M$_{\odot}$/yr. This feeding might lead to further filament collapse and formation of new cores. We suggest that the protocluster is collapsing on large scales, but the velocity signature of collapse is slow compared to pure free-fall. These data are consistent with a comparatively slow global protocluster contraction under gravity, and faster core formation within, suggesting the formation of multiple generations of stars over the protocluster lifetime., Comment: Accepted in A&A, 22 pages, 21 figures, 1 interactive figure, 4 tables
Published: 2024
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8. Benchmarking the IRDC G351.77-0.53: Gaia DR3 distance, mass distribution, and star formation content

Author: Reyes-Reyes, S. D., Stutz, A. M., Megeath, S. T., Xu, Fengwei, Álvarez-Gutiérrez, R. H., Sandoval-Garrido, N., and Liu, H. -L.
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract: While intensively studied, it remains unclear how the star formation (SF) in Infrared Dark Clouds (IRDCs) compares to that of nearby clouds. We study G351.77-0.53 (henceforth G351), a cluster-forming filamentary IRDC. We begin by characterizing its young stellar object (YSO) content. Based on the average parallax of likely members, we obtain a Gaia distance of $\sim\,2.0\pm0.14$ kpc, resolving the literature distance ambiguity. Using our Herschel-derived N(H$_2$) map, we measure a total gas mass of 10200 M$_{\odot}$ (within 11 pc$^2$) and the average line-mass profile of the entire filament, which we model as $\lambda =~1660 (w/\rm pc )^{0.62}\,\,M_{\odot}\,\rm{pc}^{-1}$. At $w < 0.63$ pc, our $\lambda$ profile is higher and has a steeper power-law index than $\lambda$ profiles extracted in Orion A and most of its substructures. Based on the YSOs inside the filament area, we estimate the SF efficiency (SFE) and SF rate (SFR). We calculate a factor of 5 incompleteness correction for our YSO catalog relative to Spitzer surveys of Orion A. The G351 SFE is $\sim 1.8$ times lower than that of Orion A and lower than the median value for local clouds. We measure SFR and gas masses to estimate the efficiency per free-fall time, $\epsilon _{\rm ff}$. We find that $\epsilon_{\rm ff}$ is $\sim$ 1.1 dex below the previously proposed mean local relation, and $\sim\,4.7\times$ below Orion A. These observations indicate that local SF-relations do not capture variations present in the Galaxy. We speculate that cloud youth and/or magnetic fields might account for the G351 inefficiency., Comment: 14 pages (13 main body; 1 appendix), 8 figures
Published: 2024
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9. ALMA-IMF XI: The sample of hot core candidates A rich population of young high-mass proto-stars unveiled by the emission of methyl formate

Author: Bonfand, M., Csengeri, T., Bontemps, S., Brouillet, N., Motte, F., Louvet, F., Ginsburg, A., Cunningham, N., Galván-Madrid, R., Herpin, F., Wyrowski, F., Valeille-Manet, M., Stutz, A. M., Di Francesco, J., Gusdorf, A., Fernández-López, M., Lefloch, B., Liu, H-L., Sanhueza, P., Álvarez-Gutiérrez, R. H., Olguin, F., Nony, T., Lopez-Sepulcre, A., Dell'Ova, P., Pouteau, Y., Jeff, D., Chen, H. -R. V., Armante, M., Towner, A., Bronfman, L., and Kessler, N.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: Sites associated with high-mass star and cluster formation exhibit a so-called hot core phase, characterized by high temperatures and column densities of complex organic molecules. We built a comprehensive census of hot core candidates towards the ALMA-IMF protoclusters based on the detection of two CH3OCHO emission lines at 216.1 GHz. We used the source extraction algorithm GExt2D to identify peaks of methyl formate (CH3OCHO) emission that is a complex species commonly observed towards sites of star formation. We built up a catalog of 76 hot core candidates with masses ranging from about 0.2 to 80 Msun , of which 56 are new detections. A large majority of these objects are compact, rather circular, with deconvolved FWHM sizes of about 2300 au on average. About 30% of our sample of methyl formate sources have core masses above 8 Msun within sizes ranging from about 1000 au to 13400 au, which well correspond to archetypical hot cores. The origin of the CH3OCHO emission toward the lower-mass cores can be explained by a mixture of contribution from shocks, or may correspond to objects in a more evolved state, i.e. beyond the hot core stage. We find that the fraction of hot core candidates increases with the core mass. The large fraction of hot core candidates towards the most massive cores suggests that they rapidly enter the hot core phase and feedback effects from the forming protostar(s) impact their environment on short time-scales.
Published: 2024
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10. ALMA-IMF X -- The core population in the evolved W33-Main (G012.80) protocluster

Author: Armante, M., Gusdorf, A., Louvet, F., Motte, F., Pouteau, Y., Lesaffre, P., Galván-Madrid, R., Dell'Ova, P., Bonfand, M., Nony, T., Brouillet, N., Cunningham, N., Ginsburg, A., Men'shchikov, A., Bontemps, S., González, D. Díaz, Csengeri, T., Fernández-López, M., González, M., Herpin, F., Liu, H. -L., Sanhueza, P., Stutz, A. M., and Valeille-Manet, M.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We aimed to measure the CMF in the evolved W33-Main star-forming protocluster to compare it with CMF recently obtained in other Galactic star-forming regions, including the ones included in the ALMA-IMF program. We used observations from the ALMA-IMF large program: 2'x2' maps of emission from the continuum and selected lines at 1.3mm and 3mm observed by the ALMA 12m only antennas. Our angular resolution was typically 1'', that is 2400au at a distance of 2.4kpc. The lines we analysed are CO(2-1), SiO(5-4), N2H+(1-0), H41alpha as well as He41alpha blended with C41alpha. We built a census of dense cores in the region, and we measured the associated CMF based on a core-dependent temperature value. We confirmed the 'evolved' status of W33-Main by identifiying three HII regions within the field, and to a lesser extent based on the number and extension of N2H+ filaments. We produced a filtered core catalog of 94 candidates, that we refined to take into account the contamination of the continuum by free-free and line emission, obtaining 80 cores with masses that range from 0.03 to 13.2Msun. We fitted the resulting high-mass end of the CMF with a single power law of the form N(log(M)) ~ M^alpha, obtaining alpha = -1.44(+0.16)(-0.22), slightly steeper but consistent with the Salpeter index. We categorized our cores in pre- and protostellar, mostly based on outlow activity and hot core nature. We found the prestellar CMF to be steeper than a Salpeter-like distribution, and the protostellar CMF to be slightly top heavy. We found a higher proportion of cores within the HII regions and their surroundings than in the rest of the field. We also found that the cores' masses were rather low (maximum mass of 13Msun).
Published: 2024
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11. Feedback from protoclusters does not significantly change the kinematic properties of the embedded dense gas structures

Author: Zhou, J. W., Dib, S., Wyrowski, F., Liu, T., Li, S. H., Sanhueza, P., Juvela, M., Xu, F. W., Liu, H. L., Baug, T., Peng, Y. P., Menten, K. M., Bronfman, L., and Lee, C. W.
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract: A total of 64 ATOMS sources at different evolutionary stages were selected to investigate the kinematics and dynamics of gas structures under feedback. We identified dense gas structures based on the integrated intensity map of H$^{13}$CO$^+$ J=1-0 emission, and then extracted the average spectra of all structures to investigate their velocity components and gas kinematics. For the scaling relations between velocity dispersion $\sigma$, effective radius $R$ and column density $N$ of all structures, $\sigma-N*R$ always has a stronger correlation compared to $\sigma-N$ and $\sigma-R$. There are significant correlations between velocity dispersion and column density, which may imply that the velocity dispersion originates from gravitational collapse, also revealed by the velocity gradients. The measured velocity gradients for dense gas structures in early-stage sources and late-stage sources are comparable, indicating gravitational collapse through all evolutionary stages. We quantitatively estimated the velocity dispersion generated by the outflows, inflows, ionized gas pressure and radiation pressure, and found that the ionized gas feedback is stronger than other feedback mechanisms. However, although feedback from HII regions is the strongest, it does not significantly affect the physical properties of the embedded dense gas structures. Combining with the conclusions in Zhou+2023 on cloud-clump scales, we suggest that although feedback from cloud to core scales will break up the original cloud complex, the substructures of the original complex can be reorganized into new gravitationally governed configurations around new gravitational centers. This process is accompanied by structural destruction and generation, and changes in gravitational centers, but gravitational collapse is always ongoing., Comment: 15 pages, accepted for publication in Astronomy & Astrophysics
Published: 2023

12. ALMA-IMF IX: Catalog and Physical Properties of 315 SiO Outflow Candidates in 15 Massive Protoclusters

Author: Towner, A. P. M., Ginsburg, A., Dell'Ova, P., Gusdorf, A., Bontemps, S., Csengeri, T., Galván-Madrid, R., Louvet, F. K., Motte, F., Sanhueza, P., Stutz, A. M., Bally, J., Baug, T., Chen, H. R. V., Cunningham, N., Fernández-López, M., Liu, H. -L., Lu, X., Nony, T., Valeille-Manet, M., Wu, B., Álvarez-Gutiérrez, R. H., Bonfand, M., Di Francesco, J., Nguyen-Luong, Q., Olguin, F., and Whitworth, A. P.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We present a catalog of 315 protostellar outflow candidates detected in SiO J=5-4 in the ALMA-IMF Large Program, observed with ~2000 au spatial resolution, 0.339 km/s velocity resolution, and 2-12 mJy/beam (0.18-0.8 K) sensitivity. We find median outflow masses, momenta, and kinetic energies of ~0.3 M$_{\odot}$, 4 M$_{\odot}$ km/s, and 10$^{45}$ erg, respectively. Median outflow lifetimes are 6,000 years, yielding median mass, momentum, and energy rates of $\dot{M}$ = 10$^{-4.4}$ M$_{\odot}$ yr$^{-1}$, $\dot{P}$ = 10$^{-3.2}$ M$_{\odot}$ km/s yr$^{-1}$, and $\dot{E}$ = 1 L$_{\odot}$. We analyze these outflow properties in the aggregate in each field. We find correlations between field-aggregated SiO outflow properties and total mass in cores (~3$-$5$\sigma$), and no correlations above 3$\sigma$ with clump mass, clump luminosity, or clump luminosity-to-mass ratio. We perform a linear regression analysis and find that the correlation between field-aggregated outflow mass and total clump mass - which has been previously described in the literature - may actually be mediated by the relationship between outflow mass and total mass in cores. We also find that the most massive SiO outflow in each field is typically responsible for only 15-30% of the total outflow mass (60% upper limit). Our data agree well with the established mechanical force-bolometric luminosity relationship in the literature, and our data extend this relationship up to L $\geq$ 10$^6$ L$_{\odot}$ and $\dot{P}$ $\geq$ 1 M$_{\odot}$ km/s yr$^{-1}$. Our lack of correlation with clump L/M is inconsistent with models of protocluster formation in which all protostars start forming at the same time., Comment: 46 pages, 14 figures, 10 tables. This publication has an associated Zenodo entry, which can be found here: https://zenodo.org/records/8350595
Published: 2023

13. ATOMS: ALMA Three-millimeter Observations of Massive Star-forming regions -XIV. Properties of resolved UC Hii regions

Author: Zhang, C., Zhu, Feng-Yao, Liu, Tie, Ren, Z. -Y., Liu, H. -L., Wang, Ke, Wu, J. -W., Zhang, Y., Zhou, J. -W., Tatematsu, K., Garay, Guido, Tej, Anandmayee, Li, Shanghuo, Xu, W. F., Lee, Chang Won, Bronfman, Leonardo, Soam, Archana, and Li, D.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: Hydrogen recombination lines (RRLs) are one of the major diagnostics of the physical properties of H{\sc ii} regions. We use RRL H40$\alpha$, He40$\alpha$ and 3 mm continuum emission to investigate the properties of a large sample of resolved UC H{\sc ii} regions identified in the ATOMS survey. In total, we identify 94 UC H{\sc ii} regions from H40$\alpha$ emission. The basic parameters for these UC H{\sc ii} regions such as electron density, emission measure, electron temperature, ionic abundance ratio (n$_{\rm He^+}$/n$_{\rm H^+}$), and line width are derived. The median electron density and the median n$_{\rm He^+}$/n$_{\rm H^+}$ ratio of these UC H{\sc ii} regions derived from RRLs are $\sim$9000 cm$^{-3}$ and 0.11, respectively. Within UC H{\sc ii} regions, the n$_{\rm He^+}$/n$_{\rm H^+}$ ratios derived from the intensity ratio of the He40$\alpha$ and H40$\alpha$ lines seems to be higher in the boundary region than in the center. The H40$\alpha$ line width is mainly broadened by thermal motion and microturbulence. The electron temperature of these UC H{\sc ii} regions has a median value of $\sim$6700 K, and its dependence on galactocentric distance is weak.
Published: 2023
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14. ALMA-IMF VI -- Investigating the origin of stellar masses: Core mass function evolution in the W43-MM2&MM3 mini-starburst

Author: Pouteau, Y., Motte, F., Nony, T., Gonzalez, M., Joncour, I., Robitaille, J. -F., Busquet, G., Galvan-Madrid, R., Gusdorf, A., Hennebelle, P., Ginsburg, A., Csengeri, T., Sanhueza, P., Dell'Ova, P., Stutz, A. M., Towner, A. P. M., Cunningham, N., Louvet, F., Men'shchikov, A., Fernandez-Lopez, M., Schneider, N., Armante, M., Bally, J., Baug, T., Bonfand, M., Bontemps, S., Bronfman, L., Brouillet, N., Diaz-Gonzalez, D., Herpin, F., Lefloch, B., Liu, H. -L., Lu, X., Nakamura, F., Luong, Q. Nguyen, Olguin, F., Tatematsu, K., and Valeille-Manet, M.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: Among the most central open questions regarding the initial mass function (IMF) of stars is the impact of environment on the shape of the core mass function (CMF) and thus potentially on the IMF. The ALMA-IMF Large Program aims to investigate the variations in the core distributions with cloud characteristics, as diagnostic observables of the formation process and evolution of clouds. The present study focuses on the W43-MM2&MM3 mini-starburst, whose CMF has recently been found to be top-heavy with respect to the Salpeter slope. W43-MM2&MM3 harbors a rich cluster that contains a statistically significant number of cores, which was previously characterized in Paper III. We applied a multi-scale decomposition technique to the ALMA 1.3 mm and 3 mm continuum images to define six subregions. For each subregion we characterized the high column density probability distribution function, n-PDF, and the shape of the cloud gas using the 1.3 mm image. Using the core catalog, we investigate correlations between the CMF and cloud and core properties. We classify the subregions into different stages of evolution, from quiescent to burst to post-burst, based on the surface number density of cores, number of outflows, and UCHii presence. The high-mass end of the subregion CMFs varies from being close to the Salpeter slope (quiescent) to top-heavy (burst and post-burst). Moreover, the second tail of the n-PDF varies from steep, to flat like observed for the high mass star-forming clouds. We found that subregions with flat second n-PDF tails display top-heavy CMFs. The CMF may evolve from Salpeter to top-heavy throughout the star formation process from the quiescent to the burst phase. This scenario raises the question of if the CMF might revert again to Salpeter as the cloud approaches the end of its star formation stage, a hypothesis that remains to be tested., Comment: Accepted for publication in A&A (december, 5th 2022) after language editing; 25 pages, 14 figures
Published: 2022
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15. ATOMS: ALMA Three-millimeter Observations of Massive Star-forming regions -- X. Chemical differentiation among the massive cores in G9.62+0.19

Author: Peng, Y. P., Liu, T., Qin, S. -L., Baug, T., Liu, H. -L., Wang, K., Garay, G., Zhang, C., Chen, L. -F., Lee, C. W., Juvela, M., Li, D. L., Tatematsu, K., Liu, X. -C., Lee, J. -E., Luo, G., Dewangan, L., Wu, Y. -F., Zhang, L., Bronfman, L., Ge, J. X., Tang, M. Y., Zhang, Y., Xu, F. -W., Wang, Y., and Zhou, B.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: Investigating the physical and chemical structures of massive star-forming regions is critical for understanding the formation and the early evolution of massive stars. We performed a detailed line survey toward six dense cores named as MM1, MM4, MM6, MM7, MM8, and MM11 in G9.62+0.19 star-forming region resolved in ALMA band 3 observations. Toward these cores, about 172 transitions have been identified and attributed to 16 species including organic Oxygen-, Nitrogen-, Sulfur-bearing molecules and their isotopologues. Four dense cores MM7, MM8, MM4, and MM11 are line rich sources. Modeling of these spectral lines reveals the rotational temperature in a range of 72$-$115~K, 100$-$163~K, 102$-$204~K, and 84$-$123~K for the MM7, MM8, MM4, and MM11, respectively. The molecular column densities are 1.6 $\times$ 10$^{15}$ $-$ 9.2 $\times$ 10$^{17}$~cm$^{-2}$ toward the four cores. The cores MM8 and MM4 show chemical difference between Oxygen- and Nitrogen-bearing species, i.e., MM4 is rich in oxygen-bearing molecules while nitrogen-bearing molecules especially vibrationally excited HC$_{3}$N lines are mainly observed in MM8. The distinct initial temperature at accretion phase may lead to this N/O differentiation. Through analyzing column densities and spatial distributions of O-bearing Complex Organic Molecules (COMs), we found that C$_{2}$H$_{5}$OH and CH$_{3}$OCH$_{3}$ might have a common precursor, CH$_{3}$OH. CH$_{3}$OCHO and CH$_{3}$OCH$_{3}$ are likely chemically linked. In addition, the observed variation in HC$_{3}$N and HC$_{5}$N emission may indicate that their different formation mechanism at hot and cold regions., Comment: 40 pages, 23 figures
Published: 2022
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16. ALMA-IMF III -- Investigating the origin of stellar masses: Top-heavy core mass function in the W43-MM2&MM3 mini-starburst

Author: Pouteau, Y., Motte, F., Nony, T., Galván-Madrid, R., Men'shchikov, A., Bontemps, S., Robitaille, J. -F., Louvet, F., Ginsburg, A., Herpin, F., López-Sepulcre, A., Dell'Ova, P., Gusdorf, A., Sanhueza, P., Stutz, A. M., Brouillet, N., Thomasson, B., Armante, M., Baug, T., Busquet, G., Csengeri, T., Cunningham, N., Fernández-López, M., Liu, H. -L., Olguin, F., Towner, A. P. M., Bally, J., Braine, J., Bronfman, L., Joncour, I., González, M., Hennebelle, P., Lu, X., Menten, K. M., Moraux, E., Tatematsu, K., Walker, D., and Whitworth, A. P.
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract: The ALMA-IMF Large Program observed the W43-MM2-MM3 ridge, whose 1.3mm and 3mm ALMA 12m array continuum images reach a 2500au spatial resolution. We used both the best-sensitivity and the line-free ALMA-IMF images, reduced the noise with the multi-resolution segmentation technique MnGSeg, and derived the most complete and most robust core catalog possible. Using two different extraction software packages, getsf and GExt2D, we identified 200 compact sources, whose 100 common sources have on average fluxes consistent to within 30%. We filtered sources with non-negligible free-free contamination and corrected fluxes from line contamination, resulting in a W43-MM2-MM3 catalog of 205 getsf cores. With a median deconvolved FWHM size of 3400au, core masses range from 0.1Msun to 70Msun and the getsf catalog is 90% complete down to 0.8Msun. The high-mass end of the core mass function (CMF) of W43-MM2-MM3 is top-heavy compared to the canonical IMF. Fitting the cumulative CMF with a single power law of the form N(>logM)\propto M^a, we measured a=-0.95\pm0.04, compared to the canonical a=-1.35 Salpeter IMF slope. The slope of the CMF is robust with respect to map processing, extraction software package, and reasonable variations in the assumptions taken to estimate core masses. We explore several assumptions on how cores transfer their mass to stars and sub-fragment to predict the IMF resulting from the W43-MM2-MM3 CMF. In stark contrast to the commonly accepted paradigm, our result argues against the universality of the CMF shape. More robust functions of the star-formation efficiency and core sub-fragmentation are required to better predict the resulting IMF, here suggested to remain top-heavy at the end of the star-formation phase. If confirmed, the IMFs emerging from starburst events could inherit their top-heavy shape from their parental CMFs, challenging the IMF universality., Comment: 28 pages, 16 figures, 6 tables, A&A accepted on 02/08/22, revised following the language referee report
Published: 2022
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17. ALMA-IMF I -- Investigating the origin of stellar masses: Introduction to the Large Program and first results

Author: Motte, F., Bontemps, S., Csengeri, T., Pouteau, Y., Louvet, F., Stutz, A. M., Cunningham, N., López-Sepulcre, A., Brouillet, N., Galván-Madrid, R., Ginsburg, A., Maud, L., Men'shchikov, A., Nakamura, F., Nony, T., Sanhueza, P., Álvarez-Gutiérrez, R. H., Armante, M., Baug, T., Bonfand, M., Busquet, G., Chapillon, E., Díaz-González, D., Fernández-López, M., Guzmán, A. E., Herpin, F., Liu, H. -L., Olguin, F., Towner, A. P. M., Bally, J., Battersby, C., Braine, J., Bronfman, L., Chen, H. -R. V., Dell'Ova, P., Di Francesco, J., González, M., Gusdorf, A., Hennebelle, P., Izumi, N., Joncour, I., Lee, Y. -N., Lefloch, B., Lesaffre, P., Lu, X., Menten, K. M., Mignon-Risse, R., Molet, J., Moraux, E., Mundy, L., Luong, Q. Nguyen, Reyes, N., Reyes, S. D. Reyes, Robitaille, J. -F., Rosolowsky, E., Sandoval-Garrido, N. A., Schuller, F., Svoboda, B., Tatematsu, K., Thomasson, B., Walker, D., Wu, B., Whitworth, A. P., and Wyrowski, F.
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract: The ALMA-IMF Large Program imaged a total noncontiguous area of 53pc2, covering 15 extreme, nearby protoclusters of the Milky Way. They were selected to span relevant early protocluster evolutionary stages. Our 1.3mm and 3mm observations provide continuum images that are homogeneously sensitive to point-like cores with masses of 0.2 and 0.6Msun, respectively, with a matched spatial resolution of 2000au. We also detect lines that probe the protocluster structure, kinematics, chemistry, and feedback over scales from clouds to filaments to cores. We classify ALMA-IMF protoclusters as Young, Intermediate, or Evolved based on the amount of dense gas in the cloud that has potentially been impacted by HII regions. The ALMA-IMF catalog contains 700 cores that span a mass range of 0.15-250Msun at a typical size of 2100au. We show that this core sample has no significant distance bias and can be used to build core mass functions at similar physical scales. Significant gas motions, which we highlight here in the G353.41 region, are traced down to core scales and can be used to look for inflowing gas streamers and to quantify the impact of the possible associated core mass growth on the shape of the CMF with time. Our first analysis does not reveal any significant evolution of the matter concentration from clouds to cores or from the youngest to more evolved protoclusters, indicating that cloud dynamical evolution and stellar feedback have for the moment only had a slight effect on the structure of high-density gas in our sample. Furthermore, the first-look analysis of the line richness toward bright cores indicates that the survey encompasses several tens of hot cores, of which we highlight the most massive in the G351.77 cloud. Their homogeneous characterization can be used to constrain the emerging molecular complexity in protostars of high to intermediate masses., Comment: 27 pages, 9 figures, accepted for publication by A&A
Published: 2021
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18. ATOMS: ALMA Three-millimeter Observations of Massive Star-forming regions -- IV. Radio Recombination Lines and evolution of star formation efficiencies

Author: Zhang, C., Evans II, Neal J., Liu, T., Wu, J. -W., Wang, Ke, Liu, H. -L., Zhu, F. -Y., Ren, Z. -Y., Dewangan, L. K., Lee, Chang Won, Li, Shanghuo, Bronfman, L., Tej, A., and Li, D.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We report detection of radio recombination line (RRL) H$_{40\alpha}$ toward 75 sources, with data obtained from ACA observations in the ATOMS survey of 146 active Galactic star forming regions. We calculated ionized gas mass and star formation rate with H40U line emission. The mass of ionized gas is significantly smaller than molecular gas mass, indicating that ionized gas is negligible in the star forming clumps of the ATOMS sample. The star formation rate (SFR$_{{\rm H}_{40\alpha}}$) estimated with RRL H$_{40\alpha}$ agrees well with that (SFR$_{\rm L_{bol}}$) calculated with the total bolometric luminosity (L$_{\rm bol}$) when SFR $\gtrsim 5 {\rm M_\odot My}r^{-1}$, suggesting that millimeter RRLs could well sample the upper part of the initial mass function (IMF) and thus be good tracers for SFR. We also study the relationships between L$_{\rm bol}$ and the molecular line luminosities (L0mol) of CS J=2-1 and HC$_3$N J=11-10 for all the 146 ATOMS sources. The Lbol-L0mol correlations of both the CS J=2-1 and HC3N J=11-10 lines appear approximately linear and these transitions have success in predicting L$_{\rm bol}$ similar to that of more commonly used transitions. The L$_{\rm bol}$-to-L$_{\rm mol}$ ratios or SFR-to-mass ratios (star formation efficiency; SFE) do not change with galactocentric distances (R$_{\rm GC}$). Sources with H$_{40\alpha}$ emission (or H$_{\rm II}$ regions) show higher L$_{\rm bol}$-to-L$_{\rm mol}$ than those without H$_{40\alpha}$ emission, which may be an evolutionary effect.
Published: 2021
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19. A search for cloud cores affected by shocked carbon chain chemistry in L1251

Author: Liu, Xunchuan, Wu, Y., Zhang, C., Chen, X., Lin, L. -H., Qin, S. -L., Liu, T., Henkel, C., Wang, J., Liu, H. -L., Yuan, J., Yuan, L. -X., Li, J., Shen, Z. -Q., Li, D., Esimbek, J., Wang, K., Li, L. -X., Kim, Kee-Tae, Zhu, L., Madones, D., Inostroza, N., Meng, F. -Y., Zhang, Tianwei, Tatematsu, K., Xu, Y., Ju, B. -G., Kraus, A., and Xu, F. -W.
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract: We searched for shocked carbon chain chemistry (SCCC) sources with C$_3$S abundances surpassing those of HC$_5$N towards the dark cloud L1251, using the Effelsberg telescope at K-band (18 -- 26\,GHz). L1251-1 and L1251-3 are identified as the most promising SCCC sources. The two sources harbor young stellar objects. We conducted mapping observations towards L1251-A, the western tail of L1251, at $\lambda$ $\sim$3\,mm with the PMO 13.7 m and the NRO 45 m telescopes in lines of C$_2$H, N$_2$H$^+$, CS, HCO$^+$, SO, HC$_3$N and C$^{18}$O as well as in CO 3--2 using the JCMT. The spectral data were combined with archival data including Spitzer and Herschel continuum maps for further analysis. Filamentary sub-structures labeled as F1 to F6 were extracted in L1251, with F1 being associated with L1251-A hosting L1251-1. The peak positions of dense gas traced by HCO$^+$ are misaligned relative to those of the dust clumps. Episodic outflows are common in this region. The twisted morphology of F1 and velocity distribution along L1251-A may originate from stellar feedback. SCCC in L1251-1 may have been caused by outflow activities originated from the infrared source IRS1. The signposts of ongoing SCCC and the broadened line widths of C$_3$S and C$_4$H in L1251-1 as well as the distribution of HC$_3$N are also related to outflow activities in this region. L1251-1 (IRS1) together with the previously identified SCCC source IRS3 demonstrate that L1251-A is an excellent region to study shocked carbon chain chemistry., Comment: 32 pages, 15 figures
Published: 2021
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20. Heavy element contributions of rotating massive stars to Interstellar Medium

Author: Wu, R. Q., Zhu, C. H., Lü, G. L., Wang, Z. J., and Liu, H. L.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: Employing the the stellar evolution code (Modules for Experiments in Stellar Astrophysics), we calculate yields of heavy elements from massive stars via stellar wind and core-collapse supernovae (CCSN) ejecta to interstellar medium (ISM). In our models, the initial masses ($M_{\rm ini}$) of massive stars are taken from 13 to 80 $M_\odot$, their initial rotational velocities (V) are 0, 300 and 500 km s$^{-1}$, and their metallicities are [Fe/H] = -3, -2, -1, and 0. The yields of heavy elements coming from stellar winds are mainly affected by the stellar rotation which changes the chemical abundances of stellar surfaces via chemically homogeneous evolution, and enhances mass-loss rate. We estimate that the stellar wind can produce heavy element yields of about $10^{-2}$ (for low metallicity models) to several $M_\odot$ (for low metallicity and rapid rotation models) mass. The yields of heavy element produced by CCSN ejecta also depend on the remnant mass of massive mass which is mainly determined by the mass of CO-core. Our models calculate that the yields of heavy elements produced by CCSN ejecta can get up to several $M_\odot$. Compared with stellar wind, CCSN ejecta has a greater contribution to the heavy elements in ISM. We also compare the $^{56}$Ni yields by calculated in this work with observational estimate. Our models only explain the $^{56}$Ni masses produced by faint SNe or normal SNe with progenitor mass lower than about 25 $M_\odot$, and greatly underestimate the $^{56}$Ni masses produced by stars with masses higher than about 30 $M_\odot$., Comment: 11 pages,9 figures
Published: 2021
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21. Determining the temperature in heavy-ion collisions with multiplicity distribution

Author: Song, Y. D., Wang, R., Ma, Y. G., Deng, X. G., and Liu, H. L.
Subjects: Nuclear Theory, High Energy Physics - Phenomenology, Nuclear Experiment
Abstract: By relating the charge multiplicity distribution and the temperature of a de-exciting nucleus through a deep neural network, we propose that the charge multiplicity distribution can be used as a thermometer of heavy-ion collisions. Based on an isospin-dependent quantum molecular dynamics model, we study the caloric curve of reaction $^{103}$Pd + $^9$Be with the apparent temperature determined through the charge multiplicity distribution. The caloric curve shows a characteristic signature of nuclear liquid-gas phase transition around the apparent temperature $T_{\rm ap}$ $=$ $6.4~\rm MeV$, which is consistent with that through a traditional heavy-ion collision thermometer, and indicates the viability of determining the temperature in heavy-ion collisions with multiplicity distribution., Comment: 7 pages, 7 figures; Physics Letters B, in press
Published: 2021
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22. Dust polarized emission observations of NGC 6334; BISTRO reveals the details of the complex but organized magnetic field structure of the high-mass star-forming hub-filament network

Author: Arzoumanian, D., Furuya, R., Hasegawa, T., Tahani, M., Sadavoy, S., Hull, C. L. H., Johnstone, D., Koch, P. M., Inutsuka, S. -i., Doi, Y., Hoang, T., Onaka, T., Iwasaki, K., Shimajiri, Y., Inoue, T., Peretto, N., André, P., Bastien, P., Berry, D., Chen, H. -R. V., Di Francesco, J., Eswaraiah, C., Fanciullo, L., Fissel, L. M., Hwang, J., Kang, J. -h., Kim, G., Kim, K. -T., Kirchschlager, F., Kwon, W., Lee, C. W., Liu, H. -L., Lyo, A. -R., Pattle, K., Soam, A., Tang, X., Whitworth, A., Ching, T. -C., Coudé, S., Wang, J. -W., Ward-Thompson, D., Lai, S. -P., Qiu, K., Bourke, T. L., Byun, D. -Y., Chen, M., Chen, Z., Chen, W. P., Cho, J., Choi, Y., Choi, M., Chrysostomou, A., Chung, E. J., Dai, S., Diep, P. N., Duan, H. -Y., Duan, Y., Eden, D., Fiege, J., Franzmann, E., Friberg, P., Fuller, G., Gledhill, T., Graves, S., Greaves, J., Griffin, M., Gu, Q., Han, I., Hatchell, J., Hayashi, S., Houde, M., Jeong, I. -G., Kang, M., Kang, S. -j., Kataoka, A., Kawabata, K., Kemper, F., Kim, M. -R., Kim, K. H., Kim, J., Kim, S., Kirk, J., Kobayashi, M. I. N., Konyves, V., Kusune, T., Kwon, J., Lacaille, K., Law, C. -Y., Lee, C. -F., Lee, Y. -H., Lee, S. -S., Lee, H., Lee, J. -E., Li, H. -b., Li, D., Liu, J., Liu, T., Liu, S. -Y., Lu, X., Mairs, S., Matsumura, M., Matthews, B., Moriarty-Schieven, G., Nagata, T., Nakamura, F., Nakanishi, H., Ngoc, N. B., Ohashi, N., Park, G., Parsons, H., Pyo, T. -S., Qian, L., Rao, R., Rawlings, J., Rawlings, M., Retter, B., Richer, J., Rigby, A., Saito, H., Savini, G., Scaife, A., Seta, M., Shinnaga, H., Tamura, M., Tang, Y. -W., Tomisaka, K., Tram, L. N., Tsukamoto, Y., Viti, S., Wang, H., Xie, J., Yen, H. -W., Yoo, H., Yuan, J., Yun, H. -S., Zenko, T., Zhang, G., Zhang, C. -P., Zhang, Y., Zhou, J., Zhu, L., de Looze, I., Dowell, C. D., Eyres, S., Falle, S., Friesen, R., Robitaille, J. -F., and van Loo, S.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: [Abridged] Filaments and hubs have received special attention recently thanks to studies showing their role in star formation. While the column density and velocity structures of both filaments and hubs have been studied, their magnetic fields (B-field) are not yet characterized. We aim to understand the role of the B-field in the dynamical evolution of the NGC 6334 hub-filament network. We present new observations of the dust polarized emission at 850$\mu$m towards NGC 6334 obtained with the JCMT/POL-2. We study the distribution and dispersion of the polarized intensity ($PI$), the polarization fraction ($PF$), and the B-field angle ($\theta_{B}$). We derive the power spectrum of the intensity and $\theta_{B}$ along the ridge crest. Our analyses show a complex B-field structure when observed over the whole region ($\sim10$ pc), however, at smaller scales ($\sim1$ pc), $\theta_{B}$ varies coherently along the filaments. The observed power spectrum of $\theta_{B}$ can be well represented with a power law function with a slope $-1.33\pm0.23$, which is $\sim20\%$ shallower than that of $I$. This result is compatible with the properties of simulated filaments and may indicate the processes at play in the formation of filaments. $\theta_{B}$ rotates from being mostly perpendicular to the filament crests to mostly parallel as they merge with the hubs. This variation of $\theta_{B}$ may be tracing local velocity flows of matter in-falling onto the hubs. Our analysis suggests a variation of the energy balance along the crests of these filaments, from magnetically critical/supercritical at their far ends to magnetically subcritical near the hubs. We detect an increase of $PF$ towards the high-column density star cluster-forming hubs that may result from the increase of grain alignment efficiency due to stellar radiation from the newborn stars., Comment: Accepted for publication in Astronomy & Astrophysics
Published: 2020
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23. Reaction rate weighted multilayer nuclear reaction network

Author: Liu, H. L., Han, D. D., Ji, P., and Ma, Y. G.
Subjects: Nuclear Theory, Nuclear Experiment
Abstract: Nuclear reaction rate ($\lambda$) is a significant factor in the process of nucleosynthesis. A multi-layer directed-weighted nuclear reaction network in which the reaction rate as the weight, and neutron, proton, $^4$He and the remainder nuclei as the criterion for different reaction-layers is for the first time built based on all thermonuclear reactions in the JINA REACLIB database. Our results show that with the increase of the stellar temperature ($T_{9}$), the distribution of nuclear reaction rates on the $R$-layer network demonstrates a transition from unimodal to bimodal distributions. Nuclei on the $R$-layer in the region of $\lambda = [1,2.5\times10^{1}]$ have a more complicated out-going degree distribution than the one in the region of $\lambda = [10^{11},10^{13}]$, and the number of involved nuclei at $T_{9} = 1$ is very different from the one at $T_{9} = 3$. The redundant nuclei in the region of $\lambda = [1, 2.5\times10^{1}]$ at $T_{9} = 3$ prefer $(\gamma,p)$ and $({\gamma,\alpha})$ reactions to the ones at $T_{9}=1$, which produce nuclei around the $\beta$ stable line. This work offers a novel way to the big-data analysis on nuclear reaction network at stellar temperatures., Comment: 6 pages, 4 figures, 2 tables
Published: 2020
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24. Network structure of thermonuclear reactions in nuclear landscape

Author: Liu, H. L., Han, D. D., Ma, Y. G., and Zhu, L.
Subjects: Nuclear Theory
Abstract: Nucleosynthesis is a complex process in astro-nuclear evolution. In this work, we construct a directed multi-layer nuclear reaction network using the substrate-product method from a thermonuclear reaction database, JINA REACLIB. The network contains four layers, namely $n$-, $p$-, $h$- and $r$, corresponding to the reaction types involved in neutrons, protons, $^4$He and the remainder, respectively. The degree values (i.e. numbers of reactions) for three layers of n-, p- and h- have a significant correlation with one another, and their topological structures exhibit a similar regularity. However, the $r$-layer has a more complex topological structure than others and has less correlation with the other three layers. A software package named `mfinder' is employed to analyze the motif structure of the nuclear reaction network. We thus identify the most frequent reaction patterns of interconnections occurring among different nuclides. This work provides a novel approach to study the nuclear reaction network prevailing in the astrophysical context., Comment: 7 pages, 6 figures
Published: 2020
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25. Thermal Transfer Effects of CRTS II Slab Track Under Various Meteorological Conditions

Author: Zhou, R., Yuan, W. H., Du, Y. D., Liu, H. L., Zhang, L. H., di Prisco, Marco, Series Editor, Chen, Sheng-Hong, Series Editor, Vayas, Ioannis, Series Editor, Kumar Shukla, Sanjay, Series Editor, Sharma, Anuj, Series Editor, Kumar, Nagesh, Series Editor, Wang, Chien Ming, Series Editor, Duan, Wenhui, editor, Zhang, Lihai, editor, and Shah, Surendra P., editor
Published: 2023
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26. Effect of Vanadium on Austenite Grain Refinement and Martensite Structure

Author: Jing, T., Ning, Y. T., Liu, H. L., Yang, B., Chen, Y., Xiao, Shengxiong, Editor-in-Chief, Bassir, David, Series Editor, Gao, Bingbing, Series Editor, Jiang, Yongchao, Series Editor, Li, Jia, Series Editor, Mazumdar, Sayantan, Series Editor, Sun, Qijun, Series Editor, Tang, Juntao, Series Editor, Xiong, Chuanyin, Series Editor, Xu, Hexiu, Series Editor, Yang, Jun, Series Editor, Zhang, Yisheng, editor, and Ma, Mingtu, editor
Published: 2023
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27. Influence of Annealing Temperatures on Microstructure and Mechanical Properties of 22MnB5 Hot Stamping Steel

Author: Yang, B., Liu, H. L., Jing, T., Chen, Y., Xiao, Shengxiong, Editor-in-Chief, Bassir, David, Series Editor, Gao, Bingbing, Series Editor, Jiang, Yongchao, Series Editor, Li, Jia, Series Editor, Mazumdar, Sayantan, Series Editor, Sun, Qijun, Series Editor, Tang, Juntao, Series Editor, Xiong, Chuanyin, Series Editor, Xu, Hexiu, Series Editor, Yang, Jun, Series Editor, Zhang, Yisheng, editor, and Ma, Mingtu, editor
Published: 2023
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28. Finite-size scaling phenomenon of nuclear liquid--gas phase transition probes

Author: Liu, H. L., Ma, Y. G., and Fang, D. Q.
Subjects: Nuclear Theory, Nuclear Experiment
Abstract: Based on the isospin-dependent quantum molecular dynamics model, finite-size scaling effects on nuclear liquid--gas phase transition probes are investigated by studying the de-excitation processes of six thermal sources of different sizes with the same initial density and similar $N/Z$. Using several probes including the total multiplicity derivative ($dM_{tot}/dT$), second moment parameter ($M_2$), intermediate mass fragment (IMF) multiplicity ($N_{IMF}$), Fisher's power-law exponent ($\tau$), and Ma's nuclear Zipf's law exponent ($\xi$), the relationship between the phase transition temperature and the source size has been established. It is observed that the phase transition temperatures obtained from the IMF multiplicity, Fisher's exponent, and Ma's nuclear Zipf's law exponent have a strong correlation with the source size. Moreover, by employing the finite-size scaling law, the critical temperature $T_c$ and the critical exponent $\nu$ have been obtained for infinite nuclear matter., Comment: 5 pages, 7 figures
Published: 2019
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29. Evidence for $Z_{c}^{\pm}$ decays into the $\rho^{\pm} \eta_{c}$ final state

Author: Ablikim, M., Achasov, M. N., Ahmed, S., Albrecht, M., Alekseev, M., Amoroso, A., An, F. F., An, Q., Bai, Y., Bakina, O., Ferroli, R. Baldini, Ban, Y., Begzsuren, K., Bennett, D. W., Bennett, J. V., Berger, N., Bertani, M., Bettoni, D., Bianchi, F., Boger, E., Boyko, I., Briere, R. A., Cai, H., Cai, X., Calcaterra, A., Cao, G. F., Cetin, S. A., Chai, J., Chang, J. F., Chang, W. L., Chelkov, G., Chen, G., Chen, H. S., Chen, J. C., Chen, M. L., Chen, P. L., Chen, S. J., Chen, X. R., Chen, Y. B., Cheng, W., Chu, X. K., Cibinetto, G., Cossio, F., Dai, H. L., Dai, J. P., Dbeyssi, A., Dedovich, D., Deng, Z. Y., Denig, A., Denysenko, I., Destefanis, M., DeMori, F., Ding, Y., Dong, C., Dong, J., Dong, L. Y., Dong, M. Y., Dou, Z. L., Du, S. X., Duan, P. F., Fang, J., Fang, S. S., Fang, Y., Farinelli, R., Fava, L., Feldbauer, F., Felici, G., Feng, C. Q., Fritsch, M., Fu, C. D., Gao, Q., Gao, X. L., Gao, Y., Gao, Y. G., Gao, Z., Garillon, B., Garzia, I., Gilman, A., Goetzen, K., Gong, L., Gong, W. X., Gradl, W., Greco, M., Gu, L. M., Gu, M. H., Gu, Y. T., Guo, A. Q., Guo, L. B., Guo, R. P., Guo, Y. P., Guskov, A., Haddadi, Z., Han, S., Hao, X. Q., Harris, F. A., He, K. L., Heinsius, F. H., Held, T., Heng, Y. K., Hou, Z. L., Hu, H. M., Hu, J. F., Hu, T., Hu, Y., Huang, G. S., Huang, J. S., Huang, X. T., Huang, X. Z., Huang, Z. L., Hussain, T., Andersson, W. Ikegami, Irshad, M., Ji, Q., Ji, Q. P., Ji, X. B., Ji, X. L., Jiang, H. L., Jiang, X. S., Jiang, X. Y., Jiao, J. B., Jiao, Z., Jin, D. P., Jin, S., Jin, Y., Johansson, T., Julin, A., Kalantar-Nayestanaki, N., Kang, X. S., Kavatsyuk, M., Ke, B. C., Keshk, I. K., Khan, T., Khoukaz, A., Kiese, P., Kiuchi, R., Kliemt, R., Koch, L., Kolcu, O. B., Kopf, B., Kuemmel, M., Kuessner, M., Kupsc, A., Kurth, M., Kühn, W., Lange, J. S., Larin, P., Lavezzi, L., Leiber, S., Leithoff, H., Li, C., Li, Cheng, Li, D. M., Li, F., Li, F. Y., Li, G., Li, H. B., Li, H. J., Li, J. C., Li, J. W., Li, K. J., Li, Kang, Li, Ke, Li, Lei, Li, P. L., Li, P. R., Li, Q. Y., Li, T., Li, W. D., Li, W. G., Li, X. L., Li, X. N., Li, X. Q., Li, Z. B., Liang, H., Liang, Y. F., Liang, Y. T., Liao, G. R., Liao, L. Z., Libby, J., Lin, C. X., Lin, D. X., Liu, B., Liu, B. J., Liu, C. X., Liu, D., Liu, D. Y., Liu, F. H., Liu, Fang, Liu, Feng, Liu, H. B., Liu, H. L., Liu, H. M., Liu, Huanhuan, Liu, Huihui, Liu, J. B., Liu, J. Y., Liu, K. Y., Liu, Ke, Liu, L. D., Liu, Q., Liu, S. B., Liu, X., Liu, Y. B., Liu, Z. A., Liu, Zhiqing, Long, Y. F., Lou, X. C., Lu, H. J., Lu, J. G., Lu, Y., Lu, Y. P., Luo, C. L., Luo, M. X., Luo, P. W., Luo, T., Luo, X. L., Lusso, S., Lyu, X. R., Ma, F. C., Ma, H. L., Ma, L. L., Ma, M. M., Ma, Q. M., Ma, X. N., Ma, X. Y., Ma, Y. M., Maas, F. E., Maggiora, M., Maldaner, S., Malik, Q. A., Mangoni, A., Mao, Y. J., Mao, Z. P., Marcello, S., Meng, Z. X., Messchendorp, J. G., Mezzadri, G., Min, J., Min, T. J., Mitchell, R. E., Mo, X. H., Mo, Y. J., Morales, C. Morales, Muchnoi, N. Yu., Muramatsu, H., Mustafa, A., Nakhoul, S., Nefedov, Y., Nerling, F., Nikolaev, I. B., Ning, Z., Nisar, S., Niu, S. L., Niu, X. Y., Olsen, S. L., Ouyang, Q., Pacetti, S., Pan, Y., Papenbrock, M., Patteri, P., Pelizaeus, M., Pellegrino, J., Peng, H. P., Peng, Z. Y., Peters, K., Pettersson, J., Ping, J. L., Ping, R. G., Pitka, A., Poling, R., Prasad, V., Qi, H. R., Qi, M., Qi, T. Y., Qian, S., Qiao, C. F., Qin, N., Qin, X. S., Qin, Z. H., Qiu, J. F., Qu, S. Q., Rashid, K. H., Redmer, C. F., Richter, M., Ripka, M., Rivetti, A., Rolo, M., Rong, G., Rosner, Ch., Sarantsev, A., Savrié, M., Schoenning, K., Shan, W., Shan, X. Y., Shao, M., Shen, C. P., Shen, P. X., Shen, X. Y., Sheng, H. Y., Shi, X., Song, J. J., Song, W. M., Song, X. Y., Sosio, S., Sowa, C., Spataro, S., Sui, F. F., Sun, G. X., Sun, J. F., Sun, L., Sun, S. S., Sun, X. H., Sun, Y. J., Sun, Y. K, Sun, Y. Z., Sun, Z. J., Sun, Z. T., Tan, Y. T, Tang, C. J., Tang, G. Y., Tang, X., Tiemens, M., Tsednee, B., Uman, I., Wang, B., Wang, B. L., Wang, C. W., Wang, D., Wang, D. Y., Wang, Dan, Wang, H. H., Wang, K., Wang, L. L., Wang, L. S., Wang, M., Wang, Meng, Wang, P., Wang, P. L., Wang, W. P., Wang, X. F., Wang, Y., Wang, Y. F., Wang, Z., Wang, Z. G., Wang, Z. Y., Wang, Zongyuan, Weber, T., Wei, D. H., Weidenkaff, P., Wen, S. P., Wiedner, U., Wolke, M., Wu, L. H., Wu, L. J., Wu, Z., Xia, L., Xia, X., Xia, Y., Xiao, D., Xiao, Y. J., Xiao, Z. J., Xie, Y. G., Xie, Y. H., Xiong, X. A., Xiu, Q. L., Xu, G. F., Xu, J. J., Xu, L., Xu, Q. J., Xu, X. P., Yan, F., Yan, L., Yan, W. B., Yan, W. C., Yan, Y. H., Yang, H. J., Yang, H. X., Yang, L., Yang, R. X., Yang, S. L., Yang, Y. H., Yang, Y. X., Yang, Yifan, Yang, Z. Q., Ye, M., Ye, M. H., Yin, J. H., You, Z. Y., Yu, B. X., Yu, C. X., Yu, J. S., Yuan, C. Z., Yuan, Y., Yuncu, A., Zafar, A. A., Zeng, Y., Zhang, B. X., Zhang, B. Y., Zhang, C. C., Zhang, D. H., Zhang, H. H., Zhang, H. Y., Zhang, J., Zhang, J. L., Zhang, J. Q., Zhang, J. W., Zhang, J. Y., Zhang, J. Z., Zhang, K., Zhang, L., Zhang, S. F., Zhang, T. J., Zhang, X. Y., Zhang, Y., Zhang, Y. H., Zhang, Y. T., Zhang, Yang, hang, YaoZ, Zhang, Yu, Zhang, Z. H., Zhang, Z. P., Zhang, Z. Y., Zhao, G., Zhao, J. W., Zhao, J. Y., Zhao, J. Z., Zhao, Lei, Zhao, Ling, Zhao, M. G., Zhao, Q., Zhao, S. J., Zhao, T. C., Zhao, Y. B., Zhao, Z. G., Zhemchugov, A., Zheng, B., Zheng, J. P., Zheng, W. J., Zheng, Y. H., Zhong, B., Zhou, L., Zhou, Q., Zhou, X., Zhou, X. K., Zhou, X. R., Zhou, X. Y., Zhou, Xiaoyu, Zhou, Xu, Zhu, A. N., Zhu, J., Zhu, K., Zhu, K. J., Zhu, S., Zhu, S. H., Zhu, X. L., Zhu, Y. C., Zhu, Y. S., Zhu, Z. A., Zhuang, J., Zou, B. S., and Zou, J. H.
Subjects: High Energy Physics - Experiment
Abstract: We study $e^{+}e^{-}$ collisions with a $\pi^{+}\pi^{-}\pi^{0}\eta_{c}$ final state using data samples collected with the BESIII detector at center-of-mass energies $\sqrt{s}=4.226$, $4.258$, $4.358$, $4.416$, and $4.600$ GeV. Evidence for the decay $\zcpm\to\rhopm\etac$ is reported with a statistical significance of $3.9\sigma$ with various systematic uncertainties taken into account at $\sqrt{s} = 4.226$ GeV, and the Born cross section times branching fraction $\sigma^{B}(\EE\to \pimp\zcpm)\times \BR(\zcpm\to\rhopm\etac)$ is measured to be $(48 \pm 11 \pm 11)\,\rm{pb}$. The $\zcpm\to \rhopm\etac$ signal is not significant at the other center-of-mass energies and the corresponding upper limits are determined. In addition, no significant signal is observed in a search for $\zcppm\to \rho^{\pm}\etac$ with the same data samples. The ratios $R_{\zc}=\BR(\zcpm\to \rho^{\pm} \etac)/\BR(\zcpm\to \pi^{\pm} \jpsi)$ and $R_{\zcp}=\BR(\zcppm\to \rho^{\pm} \etac)/\BR(\zcppm\to \pi^{\pm} \hc)$ are obtained and used to discriminate between different theoretical interpretations of the $\zcpm$ and $\zcppm$.
Published: 2019
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30. Observation of $\eta_c\to\omega\omega$ in $J/\psi\to\gamma\omega\omega$

Author: Ablikim, M., Achasov, M. N., Ahmed, S., Albrecht, M., Alekseev, M., Amoroso, A., An, F. F., An, Q., Bai, Y., Bakina, O., Ferroli, R. Baldini, Ban, Y., Begzsuren, K., Bennett, D. W., Bennett, J. V., Berger, N., Bertani, M., Bettoni, D., Bianchi, F., Boger, E., Boyko, I., Briere, R. A., Cai, H., Cai, X., Calcaterra, A., Cao, G. F., Cetin, S. A., Chai, J., Chang, J. F., Chang, W. L., Chelkov, G., Chen, G., Chen, H. S., Chen, J. C., Chen, M. L., Chen, S. J., Chen, X. R., Chen, Y. B., Cheng, W., Chu, X. K., Cibinetto, G., Cossio, F., Dai, H. L., Dai, J. P., Dbeyssi, A., Dedovich, D., Deng, Z. Y., Denig, A., Denysenko, I., Destefanis, M., De Mori, F., Ding, Y., Dong, C., Dong, J., Dong, L. Y., Dong, M. Y., Dou, Z. L., Du, S. X., Fan, J. Z., Fang, J., Fang, S. S., Fang, Y., Farinelli, R., Fava, L., Feldbauer, F., Felici, G., Feng, C. Q., Fritsch, M., Fu, C. D., Gao, Q., Gao, X. L., Gao, Y., Gao, Y. G., Gao, Z., Garillon, B., Garzia, I., Gilman, A., Goetzen, K., Gong, L., Gong, W. X., Gradl, W., Greco, M., Gu, L. M., Gu, M. H., Gu, Y. T., Guo, A. Q., Guo, L. B., Guo, R. P., Guo, Y. P., Guskov, A., Han, S., Hao, X. Q., Harris, F. A., He, K. L., Heinsius, F. H., Held, T., Heng, Y. K., Hou, Z. L., Hu, H. M., Hu, J. F., Hu, T., Hu, Y., Huang, G. S., Huang, J. S., Huang, X. T., Huang, X. Z., Huang, Z. L., Hussain, T., Hüsken, N., Andersson, W. Ikegami, Imoehl, W., Irshad, M., Ji, Q., Ji, Q. P., Ji, X. B., Ji, X. L., Jiang, H. L., Jiang, X. S., Jiang, X. Y., Jiao, J. B., Jiao, Z., Jin, D. P., Jin, S., Jin, Y., Johansson, T., Kalantar-Nayestanaki, N., Kang, X. S., Kavatsyuk, M., Ke, B. C., Keshk, I. K., Khan, T., Khoukaz, A., Kiese, P., Kiuchi, R., Kliemt, R., Koch, L., Kolcu, O. B., Kopf, B., Kuemmel, M., Kuessner, M., Kupsc, A., Kurth, M., Kühn, W., Lange, J. S., Larin, P., Lavezzi, L., Leiber, S., Leithoff, H., Li, C., Li, Cheng, Li, D. M., Li, F., Li, F. Y., Li, G., Li, H. B., Li, H. J., Li, J. C., Li, J. W., Li, K. J., Li, Kang, Li, Ke, Li, L. K., Li, Lei, Li, P. L., Li, P. R., Li, Q. Y., Li, W. D., Li, W. G., Li, X. L., Li, X. N., Li, X. Q., Li, Z. B., Liang, H., Liang, Y. F., Liang, Y. T., Liao, G. R., Liao, L. Z., Libby, J., Lin, C. X., Lin, D. X., Liu, B., Liu, B. J., Liu, C. X., Liu, D., Liu, D. Y., Liu, F. H., Liu, Fang, Liu, Feng, Liu, H. B., Liu, H. L, Liu, H. M., Liu, Huanhuan, Liu, Huihui, Liu, J. B., Liu, J. Y., Liu, K. Y., Liu, Ke, Liu, L. D., Liu, Q., Liu, S. B., Liu, X., Liu, Y. B., Liu, Z. A., Liu, Zhiqing, Long, Y. F., Lou, X. C., Lu, H. J., Lu, J. G., Lu, Y., Lu, Y. P., Luo, C. L., Luo, M. X., Luo, P. W., Luo, T., Luo, X. L., Lusso, S., Lyu, X. R., Ma, F. C., Ma, H. L., Ma, L. L., Ma, M. M., Ma, Q. M., Ma, X. N., Ma, X. Y., Ma, Y. M., Maas, F. E., Maggiora, M., Maldaner, S., Malik, Q. A., Mangoni, A., Mao, Y. J., Mao, Z. P., Marcello, S., Meng, Z. X., Messchendorp, J. G., Mezzadri, G., Min, J., Min, T. J., Mitchell, R. E., Mo, X. H., Mo, Y. J., Morales, C. Morales, Muchnoi, N. Yu., Muramatsu, H., Mustafa, A., Nakhoul, S., Nefedov, Y., Nerling, F., Nikolaev, I. B., Ning, Z., Nisar, S., Niu, S. L., Niu, X. Y., Olsen, S. L., Ouyang, Q., Pacetti, S., Pan, Y., Papenbrock, M., Patteri, P., Pelizaeus, M., Pellegrino, J., Peng, H. P., Peng, Z. Y., Peters, K., Pettersson, J., Ping, J. L., Ping, R. G., Pitka, A., Poling, R., Prasad, V., Qi, M., Qi, T. Y., Qian, S., Qiao, C. F., Qin, N., Qin, X. S., Qin, Z. H., Qiu, J. F., Qu, S. Q., Rashid, K. H., Redmer, C. F., Richter, M., Ripka, M., Rivetti, A., Rolo, M., Rong, G., Rosner, Ch., Rump, M., Sarantsev, A., Savrié, M., Schoenning, K., Shan, W., Shan, X. Y., Shao, M., Shen, C. P., Shen, P. X., Shen, X. Y., Sheng, H. Y., Shi, X., Shi, X. D, Song, J. J., Song, Q. Q., Song, X. Y., Sosio, S., Sowa, C., Spataro, S., Sui, F. F., Sun, G. X., Sun, J. F., Sun, L., Sun, S. S., Sun, X. H., Sun, Y. J., Sun, Y. K, Sun, Y. Z., Sun, Z. J., Sun, Z. T., Tan, Y. T, Tang, C. J., Tang, G. Y., Tang, X., Tsednee, B., Uman, I., Wang, B., Wang, B. L., Wang, C. W., Wang, D., Wang, D. Y., Wang, H. H., Wang, K., Wang, L. L., Wang, L. S., Wang, M., Wang, Meng, Wang, P., Wang, P. L., Wang, W. P., Wang, X. F., Wang, Y., Wang, Y. F., Wang, Z., Wang, Z. G., Wang, Z. Y., Wang, Zongyuan, Weber, T., Wei, D. H., Weidenkaff, P., Wen, S. P., Wiedner, U., Wolke, M., Wu, L. H., Wu, L. J., Wu, Z., Xia, L., Xia, Y., Xiao, Y. J., Xiao, Z. J., Xie, Y. G., Xie, Y. H., Xiong, X. A., Xiu, Q. L., Xu, G. F., Xu, J. J., Xu, L., Xu, Q. J., Xu, X. P., Yan, F., Yan, L., Yan, W. B., Yan, W. C., Yan, Y. H., Yang, H. J., Yang, H. X., Yang, L., Yang, R. X., Yang, S. L., Yang, Y. H., Yang, Y. X., Yang, Yifan, Yang, Z. Q., Ye, M., Ye, M. H., Yin, J. H., You, Z. Y., Yu, B. X., Yu, C. X., Yu, J. S., Yuan, C. Z., Yuan, Y., Yuncu, A., Zafar, A. A., Zeng, Y., Zhang, B. X., Zhang, B. Y., Zhang, C. C., Zhang, D. H., Zhang, H. H., Zhang, H. Y., Zhang, J., Zhang, J. L., Zhang, J. Q., Zhang, J. W., Zhang, J. Y., Zhang, J. Z., Zhang, K., Zhang, L., Zhang, S. F., Zhang, T. J., Zhang, X. Y., Zhang, Y., Zhang, Y. H., Zhang, Y. T., Zhang, Yang, Zhang, Yao, Zhang, Yu, Zhang, Z. H., Zhang, Z. P., Zhang, Z. Y., Zhao, G., Zhao, J. W., Zhao, J. Y., Zhao, J. Z., Zhao, Lei, Zhao, Ling, Zhao, M. G., Zhao, Q., Zhao, S. J., Zhao, T. C., Zhao, Y. B., Zhao, Z. G., Zhemchugov, A., Zheng, B., Zheng, J. P., Zheng, Y. H., Zhong, B., Zhou, L., Zhou, Q., Zhou, X., Zhou, X. K., Zhou, X. R., Zhou, Xiaoyu, Zhou, Xu, Zhu, A. N., Zhu, J., Zhu, K., Zhu, K. J., Zhu, S. H., Zhu, X. L., Zhu, Y. C., Zhu, Y. S., Zhu, Z. A., Zhuang, J., Zou, B. S., and Zou, J. H.
Subjects: High Energy Physics - Experiment
Abstract: Using a sample of $(1310.6\pm7.0)\times10^6$ $J/\psi$ events recorded with the BESIII detector at the symmetric electron positron collider BEPCII, we report the observation of the decay of the $(1^1 S_0)$ charmonium state $\eta_c$ into a pair of $\omega$ mesons in the process $J/\psi\to\gamma\omega\omega$. The branching fraction is measured for the first time to be $\mathcal{B}(\eta_c\to\omega\omega)= (2.88\pm0.10\pm0.46\pm0.68)\times10^{-3}$, where the first uncertainty is statistical, the second systematic and the third is from the uncertainty of $\mathcal{B}(J/\psi\to\gamma\eta_c)$. The mass and width of the $\eta_c$ are determined as $M=(2985.9\pm0.7\pm2.1)\,$MeV/$c^2$ and $\Gamma=(33.8\pm1.6\pm4.1)\,$MeV., Comment: 13 pages, 6 figures
Published: 2019
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31. Measurements of the branching fractions of $\eta_c\to K^+K^-\pi^0$, $K^0_S K^{\pm}\pi^{\mp}$,$2(\pi^+\pi^-\pi^0)$, and $p \bar{p}$

Author: Ablikim, M., Achasov, M. N., Ahmed, S., Albrecht, M., Alekseev, M., Amoroso, A., An, F. F., An, Q., Bai, Y., Bakina, O., Ferroli, R. Baldini, Ban, Y., Begzsuren, K., Bennett, D. W., Bennett, J. V., Berger, N., Bertani, M., Bettoni, D., Bianchi, F., Bloms, J., Boyko, I., Briere, R. A., Cai, H., Cai, X., Calcaterra, A., Cao, G. F., Cetin, S. A., Chai, J., Chang, J. F., Chang, W. L., Chelkov, G., Chen, G., Chen, H. S., Chen, J. C., Chen, M. L., Chen, S. J., Chen, Y. B., Cheng, W., Cibinetto, G., Cossio, F., Dai, H. L., Dai, J. P., Dbeyssi, A., Dedovich, D., Deng, Z. Y., Denig, A., Denysenko, I., Destefanis, M., De Mori, F., Ding, Y., Dong, C., Dong, J., Dong, L. Y., Dong, M. Y., Dou, Z. L., Du, S. X., Fan, J. Z., Fang, J., Fang, S. S., Fang, Y., Farinelli, R., Fava, L., Feldbauer, F., Felici, G., Feng, C. Q., Fritsch, M., Fu, C. D., Fu, Y., Gao, Q., Gao, X. L., Gao, Y., Gao, Y. G., Gao, Z., Garillon, B., Garzia, I., Gilman, A., Goetzen, K., Gong, L., Gong, W. X., Gradl, W., Greco, M., Gu, L. M., Gu, M. H., Gu, Y. T., Guo, A. Q., Guo, L. B., Guo, R. P., Guo, Y. P., Guskov, A., Han, S., Hao, X. Q., Harris, F. A., He, K. L., Heinsius, F. H., Held, T., Heng, Y. K., Hou, Z. L., Hu, H. M., Hu, J. F., Hu, T., Hu, Y., Huang, G. S., Huang, J. S., Huang, X. T., Huang, X. Z., Huang, Z. L., Hussain, T., Hüsken, N., Andersson, W. Ikegami, Imoehl, W., Irshad, M., Ji, Q., Ji, Q. P., Ji, X. B., Ji, X. L., Jiang, H. L., Jiang, X. S., Jiang, X. Y., Jiao, J. B., Jiao, Z., Jin, D. P., Jin, S., Jin, Y., Johansson, T., Kalantar-Nayestanaki, N., Kang, X. S., Kavatsyuk, M., Ke, B. C., Keshk, I. K., Khoukaz, A., Kiese, P., Kiuchi, R., Kliemt, R., Koch, L., Kolcu, O. B., Kopf, B., Kuemmel, M., Kuessner, M., Kupsc, A., Kurth, M., Kühn, W., Lange, J. S., Larin, P., Lavezzi, L., Leithoff, H., Li, C., Li, Cheng, Li, D. M., Li, F., Li, F. Y., Li, G., Li, H. B., Li, H. J., Li, J. C., Li, J. W., Li, Ke, Li, L. K., Li, Lei, Li, P. L., Li, P. R., Li, Q. Y., Li, W. D., Li, W. G., Li, X. L., Li, X. N., Li, X. Q., Li, X. H., Li, Z. B., Liang, H., Liang, Y. F., Liang, Y. T., Liao, G. R., Liao, L. Z., Libby, J., Lin, C. X., Lin, D. X., Liu, B., Liu, B. J., Liu, C. X., Liu, D., Liu, D. Y., Liu, F. H., Liu, Fang, Liu, Feng, Liu, H. B., Liu, H. L, Liu, H. M., Liu, Huanhuan, Liu, Huihui, Liu, J. B., Liu, J. Y., Liu, K. Y., Liu, Ke, Liu, Q., Liu, S. B., Liu, X., Liu, Y. B., Liu, Z. A., Liu, Zhiqing, Long, Y. F., Lou, X. C., Lu, H. J., Lu, J. D., Lu, J. G., Lu, Y., Lu, Y. P., Luo, C. L., Luo, M. X., Luo, P. W., Luo, T., Luo, X. L., Lusso, S., Lyu, X. R., Ma, F. C., Ma, H. L., Ma, L. L., Ma, M. M., Ma, Q. M., Ma, X. N., Ma, X. X., Ma, X. Y., Ma, Y. M., Maas, F. E., Maggiora, M., Maldaner, S., Malik, Q. A., Mangoni, A., Mao, Y. J., Mao, Z. P., Marcello, S., Meng, Z. X., Messchendorp, J. G., Mezzadri, G., Min, J., Min, T. J., Mitchell, R. E., Mo, X. H., Mo, Y. J., Morales, C. Morales, Muchnoi, N. Yu., Muramatsu, H., Mustafa, A., Nakhoul, S., Nefedov, Y., Nerling, F., Nikolaev, I. B., Ning, Z., Nisar, S., Niu, S. L., Olsen, S. L., Ouyang, Q., Pacetti, S., Pan, Y., Papenbrock, M., Patteri, P., Pelizaeus, M., Peng, H. P., Peters, K., Pettersson, J., Ping, J. L., Ping, R. G., Pitka, A., Poling, R., Prasad, V., Qi, M., Qi, T. Y., Qian, S., Qiao, C. F., Qin, N., Qin, X. S., Qin, Z. H., Qiu, J. F., Qu, S. Q., Rashid, K. H., Redmer, C. F., Richter, M., Ripka, M., Rivetti, A., Rolo, M., Rong, G., Rosner, Ch., Rump, M., Sarantsev, A., Savrié, M., Schoenning, K., Shan, W., Shan, X. Y., Shao, M., Shen, C. P., Shen, P. X., Shen, X. Y., Sheng, H. Y., Shi, X., Shi, X. D, Song, J. J., Song, Q. Q., Song, X. Y., Sosio, S., Sowa, C., Spataro, S., Sui, F. F., Sun, G. X., Sun, J. F., Sun, L., Sun, S. S., Sun, X. H., Sun, Y. J., Sun, Y. K, Sun, Y. Z., Sun, Z. J., Sun, Z. T., Tan, Y. T, Tang, C. J., Tang, G. Y., Tang, X., Tsednee, B., Uman, I., Wang, B., Wang, B. L., Wang, C. W., Wang, D. Y., Wang, H. H., Wang, K., Wang, L. L., Wang, L. S., Wang, M., Wang, Meng, Wang, P., Wang, P. L., Wang, R. M., Wang, W. P., Wang, X., Wang, X. F., Wang, Y., Wang, Y. F., Wang, Z., Wang, Z. G., Wang, Z. Y., Wang, Zongyuan, Weber, T., Wei, D. H., Weidenkaff, P., Wen, S. P., Wiedner, U., Wolke, M., Wu, L. H., Wu, L. J., Wu, Z., Xia, L., Xia, Y., Xiao, Y. J., Xiao, Z. J., Xie, Y. G., Xie, Y. H., Xiong, X. A., Xiu, Q. L., Xu, G. F., Xu, L., Xu, Q. J., Xu, W., Xu, X. P., Yan, F., Yan, L., Yan, W. B., Yan, W. C., Yan, Y. H., Yang, H. J., Yang, H. X., Yang, L., Yang, R. X., Yang, S. L., Yang, Y. H., Yang, Y. X., Yang, Yifan, Yang, Z. Q., Ye, M., Ye, M. H., Yin, J. H., You, Z. Y., Yu, B. X., Yu, C. X., Yu, J. S., Yuan, C. Z., Yuan, Y., Yuncu, A., Zafar, A. A., Zeng, Y., Zhang, B. X., Zhang, B. Y., Zhang, C. C., Zhang, D. H., Zhang, H. H., Zhang, H. Y., Zhang, J., Zhang, J. L., Zhang, J. Q., Zhang, J. W., Zhang, J. Y., Zhang, J. Z., Zhang, K., Zhang, L., Zhang, S. F., Zhang, T. J., Zhang, X. Y., Zhang, Y., Zhang, Y. H., Zhang, Y. T., Zhang, Yang, Zhang, Yao, Zhang, Yu, Zhang, Z. H., Zhang, Z. P., Zhang, Z. Y., Zhao, G., Zhao, J. W., Zhao, J. Y., Zhao, J. Z., Zhao, Lei, Zhao, Ling, Zhao, M. G., Zhao, Q., Zhao, S. J., Zhao, T. C., Zhao, Y. B., Zhao, Z. G., Zhemchugov, A., Zheng, B., Zheng, J. P., Zheng, Y., Zheng, Y. H., Zhong, B., Zhou, L., Zhou, Q., Zhou, X., Zhou, X. K., Zhou, X. R., Zhou, Xiaoyu, Zhou, Xu, Zhu, A. N., Zhu, J., Zhu, K., Zhu, K. J., Zhu, S. H., Zhu, X. L., Zhu, Y. C., Zhu, Y. S., Zhu, Z. A., Zhuang, J., Zou, B. S., and Zou, J. H.
Subjects: High Energy Physics - Experiment
Abstract: Using data samples collected with the BESIII detector at center-of-mass energies $\sqrt{s} = 4.23, 4.26, 4.36,$ and $4.42$~\rm{GeV}, we measure the branching fractions of $\eta_c\to K^+K^-\pi^0$, $K^0_S K^{\pm}\pi^{\mp}$, $2(\pi^+\pi^-\pi^0)$, and $p \bar{p}$, via the process $e^+e^-\to\pi^+\pi^-h_c$, $h_c\to\gamma\eta_c$. The corresponding results are $(1.15\pm0.12\pm0.10)\%$, $(2.60\pm0.21\pm0.20)\%$, $(15.2\pm1.8\pm1.7)\%$, and $(0.120\pm0.026\pm0.015)\%$, respectively. Here the first uncertainties are statistical, and the second ones systematic. Additionally, the charged track multiplicity of $\eta_c$ decays is measured for the first time.
Published: 2019
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32. SCOPE: SCUBA-2 Continuum Observations of Pre-protostellar Evolution - Survey Description and Compact Source Catalogue

Author: Eden, D. J., Liu, Tie, Kim, Kee-Tae, Liu, S. -Y., Tatematsu, K., Di Francesco, J., Wang, K., Wu, Y., Thompson, M. A., Fuller, G. A., Li, Di, Ristorcelli, I., Kang, Sung-ju, Hirano, N., Johnstone, D., Lin, Y., He, J. H., Koch, P. M., Sanhueza, Patricio, Qin, S. -L., Zhang, Q., Goldsmith, P. F., Evans II, N. J., Yuan, J., Zhang, C. -P., White, G. J., Choi, Minho, Lee, Chang Won, Toth, L. V., Mairs, S., Yi, H. -W., Tang, M., Soam, A., Peretto, N., Samal, M. R., Fich, M., Parsons, H., Malinen, J., Bendo, G. J., Rivera-Ingraham, A., Liu, H. -L., Wouterloot, J., Li, P. S., Qian, L., Rawlings, J., Rawlings, M. G., Feng, S., Wang, B., Li, Dalei, Liu, M., Luo, G., Marston, A. P., Pattle, K. M., Pelkonen, V. -M., Rigby, A. J., Zahorecz, S., Zhang, G., Bogner, R., Aikawa, Y., Akhter, S., Alina, D., Bell, G., Bernard, J. -P., Blain, A., Bronfman, L., Byun, D. -Y., Chapman, S., Chen, H. -R., Chen, M., Chen, W. -P., Chen, X., Chen, Xuepeng, Chrysostomou, A., Chu, Y. -H., Chung, E. J., Cornu, D., Cosentino, G., Cunningham, M. R., Demyk, K., Drabek-Maunder, E., Doi, Y., Eswaraiah, C., Falgarone, E., Feher, O., Fraser, H., Friberg, P., Garay, G., Ge, J. X., Gear, W. K., Greaves, J., Guan, X., Harvey-Smith, L., Hasegawa, T., He, Y., Henkel, C., Hirota, T., Holland, W., Hughes, A., Jarken, E., Ji, T. -G., Jimenez-Serra, I., Kang, Miju, Kawabata, K. S., Kim, Gwanjeong, Kim, Jungha, Kim, Jongsoo, Kim, S., Koo, B. -C., Kwon, Woojin, Kuan, Y. -J., Lacaille, K. M., Lai, S. -P., Lee, C. F., Lee, J. E., Lee, Y. -U., Li, H., Lo, N., Lopez, J. A. P., Lu, X., Lyo, A. -R., Mardones, D., McGehee, P., Meng, F., Montier, L., Montillaud, J., Moore, T. J. T., Morata, O., Moriarty-Schieven, G. H., Ohashi, S., Pak, S., Park, Geumsook, Paladini, R., Pech, G., Qiu, K., Ren, Z. -Y., Richer, J., Sakai, T., Shang, H., Shinnaga, H., Stamatellos, D., Tang, Y. -W., Traficante, A., Vastel, C., Viti, S., Walsh, A., Wang, H., Wang, J., Ward-Thompson, D., Whitworth, A., Wilson, C. D., Xu, Y., Yang, J., Yuan, Y. -L., Yuan, L., Zavagno, A., Zhang, C., Zhang, H. -W., Zhou, C., Zhu, J. Zhou. L., and Zuo, P.
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract: We present the first release of the data and compact-source catalogue for the JCMT Large Program SCUBA-2 Continuum Observations of Pre-protostellar Evolution (SCOPE). SCOPE consists of 850-um continuum observations of 1235 Planck Galactic Cold Clumps (PGCCs) made with the Submillimetre Common-User Bolometer Array 2 on the James Clerk Maxwell Telescope. These data are at an angular resolution of 14.4 arcsec, significantly improving upon the 353-GHz resolution of Planck at 5 arcmin, and allowing for a catalogue of 3528 compact sources in 558 PGCCs. We find that the detected PGCCs have significant sub-structure, with 61 per cent of detected PGCCs having 3 or more compact sources, with filamentary structure also prevalent within the sample. A detection rate of 45 per cent is found across the survey, which is 95 per cent complete to Planck column densities of $N_{H_{2}}$ $>$ 5 $\times$ 10$^{21}$ cm$^{-2}$. By positionally associating the SCOPE compact sources with YSOs, the star formation efficiency, as measured by the ratio of luminosity to mass, in nearby clouds is found to be similar to that in the more distant Galactic Plane, with the column density distributions also indistinguishable from each other., Comment: 16 pages, 13 figures, 1 table. Accepted for publication in MNRAS
Published: 2019
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33. Precision measurement of the branching fractions of $\eta^\prime$ decays

Author: Ablikim, M., Achasov, M. N., Ahmed, S., Albrecht, M., Alekseev, M., Amoroso, A., An, F. F., An, Q., Bai, Y., Bakina, O., Ferroli, R. Baldini, Ban, Y., Begzsuren, K., Bennett, D. W., Bennett, J. V., Berger, N., Bertani, M., Bettoni, D., Bianchi, F., Boger, E., Boyko, I., Briere, R. A., Cai, H., Cai, X., Calcaterra, A., Cao, G. F., Cetin, S. A., Chai, J., Chang, J. F., Chang, W. L., Chelkov, G., Chen, G., Chen, H. S., Chen, J. C., Chen, M. L., Chen, P. L., Chen, S. J., Chen, X. R., Chen, Y. B., Cheng, W., Chu, X. K., Cibinetto, G., Cossio, F., Dai, H. L., Dai, J. P., Dbeyssi, A., Dedovich, D., Deng, Z. Y., Denig, A., Denysenko, I., Destefanis, M., De Mori, F., Ding, Y., Dong, C., Dong, J., Dong, L. Y., Dong, M. Y., Dou, Z. L., Du, S. X., Duan, P. F., Fan, J. Z., Fang, J., Fang, S. S., Fang, Y., Farinelli, R., Fava, L., Feldbauer, F., Felici, G., Feng, C. Q., Fritsch, M., Fu, C. D., Gao, Q., Gao, X. L., Gao, Y., Gao, Y. G., Gao, Z., Garillon, B., Garzia, I., Gilman, A., Goetzen, K., Gong, L., Gong, W. X., Gradl, W., Greco, M., Gu, L. M., Gu, M. H., Gu, Y. T., Guo, A. Q., Guo, L. B., Guo, R. P., Guo, Y. P., Guskov, A., Haddadi, Z., Han, S., Hao, X. Q., Harris, F. A., He, K. L., Heinsius, F. H., Held, T., Heng, Y. K., Hou, Z. L., Hu, H. M., Hu, J. F., Hu, T., Hu, Y., Huang, G. S., Huang, J. S., Huang, X. T., Huang, X. Z., Huang, Z. L., Hussain, T., Andersson, W. Ikegami, Imoehl, W., Irshad, M., Ji, Q., Ji, Q. P., Ji, X. B., Ji, X. L., Jiang, H. L., Jiang, X. S., Jiang, X. Y., Jiao, J. B., Jiao, Z., Jin, D. P., Jin, S., Jin, Y., Johansson, T., Kalantar-Nayestanaki, N., Kang, X. S., Kavatsyuk, M., Ke, B. C., Keshk, I. K., Khan, T., Khoukaz, A., Kiese, P., Kiuchi, R., Kliemt, R., Koch, L., Kolcu, O. B., Kopf, B., Kuemmel, M., Kuessner, M., Kupsc, A., Kurth, M., Kühn, W., Lange, J. S., Larin, P., Lavezzi, L., Leiber, S., Leithoff, H., Li, C., Li, Cheng, Li, D. M., Li, F., Li, F. Y., Li, G., Li, H. B., Li, H. J., Li, J. C., Li, J. W., Li, K. J., Li, Kang, Li, Ke, Li, L. K., Li, Lei, Li, P. L., Li, P. R., Li, Q. Y., Li, T., Li, W. D., Li, W. G., Li, X. L., Li, X. N., Li, X. Q., Li, Z. B., Liang, H., Liang, Y. F., Liang, Y. T., Liao, G. R., Liao, L. Z., Libby, J., Lin, C. X., Lin, D. X., Liu, B., Liu, B. J., Liu, C. X., Liu, D., Liu, D. Y., Liu, F. H., Liu, Fang, Liu, Feng, Liu, H. B., Liu, H. L., Liu, H. M., Liu, Huanhuan, Liu, Huihui, Liu, J. B., Liu, J. Y., Liu, K. Y., Liu, Ke, Liu, L. D., Liu, Q., Liu, S. B., Liu, X., Liu, Y. B., Liu, Z. A., Liu, Zhiqing, Long, Y. F., Lou, X. C., Lu, H. J., Lu, J. G., Lu, Y., Lu, Y. P., Luo, C. L., Luo, M. X., Luo, P. W., Luo, T., Luo, X. L., Lusso, S., Lyu, X. R., Ma, F. C., Ma, H. L., Ma, L. L., Ma, M. M., Ma, Q. M., Ma, X. N., Ma, X. Y., Ma, Y. M., Maas, F. E., Maggiora, M., Maldaner, S., Malik, Q. A., Mangoni, A., Mao, Y. J., Mao, Z. P., Marcello, S., Meng, Z. X., Messchendorp, J. G., Mezzadri, G., Min, J., Min, T. J., Mitchell, R. E., Mo, X. H., Mo, Y. J., Morales, C. Morales, Muchnoi, N. Yu., Muramatsu, H., Mustafa, A., Nakhoul, S., Nefedov, Y., Nerling, F., Nikolaev, I. B., Ning, Z., Nisar, S., Niu, S. L., Niu, X. Y., Olsen, S. L., Ouyang, Q., Pacetti, S., Pan, Y., Papenbrock, M., Patteri, P., Pelizaeus, M., Pellegrino, J., Peng, H. P., Peng, Z. Y., Peters, K., Pettersson, J., Ping, J. L., Ping, R. G., Pitka, A., Poling, R., Prasad, V., Qi, H. R., Qi, M., Qi, T. Y., Qian, S., Qiao, C. F., Qin, N., Qin, X. S., Qin, Z. H., Qiu, J. F., Qu, S. Q., Rashid, K. H., Redmer, C. F., Richter, M., Ripka, M., Rivetti, A., Rolo, M., Rong, G., Rosner, Ch., Sarantsev, A., Savrié, M., Schoenning, K., Shan, W., Shan, X. Y., Shao, M., Shen, C. P., Shen, P. X., Shen, X. Y., Sheng, H. Y., Shi, X., Song, J. J., Song, W. M., Song, X. Y., Sosio, S., Sowa, C., Spataro, S., Sui, F. F., Sun, G. X., Sun, J. F., Sun, L., Sun, S. S., Sun, X. H., Sun, Y. J., Sun, Y. K, Sun, Y. Z., Sun, Z. J., Sun, Z. T., Tan, Y. T, Tang, C. J., Tang, G. Y., Tang, X., Tiemens, M., Tsednee, B., Uman, I., Wang, B., Wang, B. L., Wang, C. W., Wang, D., Wang, D. Y., Wang, H. H., Wang, K., Wang, L. L., Wang, L. S., Wang, M., Wang, Meng, Wang, P., Wang, P. L., Wang, W. P., Wang, X. F., Wang, Y., Wang, Y. F., Wang, Y. Q., Wang, Z., Wang, Z. G., Wang, Z. Y., Wang, Zongyuan, Weber, T., Wei, D. H., Weidenkaff, P., Wen, S. P., Wiedner, U., Wolke, M., Wu, L. H., Wu, L. J., Wu, Z., Xia, L., Xia, X., Xia, Y., Xiao, D., Xiao, Y. J., Xiao, Z. J., Xie, Y. G., Xie, Y. H., Xiong, X. A., Xiu, Q. L., Xu, G. F., Xu, J. J., Xu, L., Xu, Q. J., Xu, X. P., Yan, F., Yan, L., Yan, W. B., Yan, W. C., Yan, Y. H., Yang, H. J., Yang, H. X., Yang, L., Yang, R. X., Yang, S. L., Yang, Y. H., Yang, Y. X., Yang, Yifan, Yang, Z. Q., Ye, M., Ye, M. H., Yin, J. H., You, Z. Y., Yu, B. X., Yu, C. X., Yu, J. S., Yuan, C. Z., Yuan, Y., Yuncu, A., Zafar, A. A., Zeng, Y., Zhang, B. X., Zhang, B. Y., Zhang, C. C., Zhang, D. H., Zhang, H. H., Zhang, H. Y., Zhang, J., Zhang, J. L., Zhang, J. Q., Zhang, J. W., Zhang, J. Y., Zhang, J. Z., Zhang, K., Zhang, L., Zhang, S. F., Zhang, T. J., Zhang, X. Y., Zhang, Y., Zhang, Y. H., Zhang, Y. T., Zhang, Yang, Zhang, Yao, Zhang, Yu, Zhang, Z. H., Zhang, Z. P., Zhang, Z. Y., Zhao, G., Zhao, J. W., Zhao, J. Y., Zhao, J. Z., Zhao, Lei, Zhao, Ling, Zhao, M. G., Zhao, Q., Zhao, S. J., Zhao, T. C., Zhao, Y. B., Zhao, Z. G., Zhemchugov, A., Zheng, B., Zheng, J. P., Zheng, W. J., Zheng, Y. H., Zhong, B., Zhou, L., Zhou, Q., Zhou, X., Zhou, X. K., Zhou, X. R., Zhou, X. Y., Zhou, Xiaoyu, Zhou, Xu, Zhu, A. N., Zhu, J., Zhu, K., Zhu, K. J., Zhu, S., Zhu, S. H., Zhu, X. L., Zhu, Y. C., Zhu, Y. S., Zhu, Z. A., Zhuang, J., Zou, B. S., and Zou, J. H.
Subjects: High Energy Physics - Experiment
Abstract: Based on a sample of $(1310.6 \pm 7.0) \times 10^6~J/\psi$ events collected with the BESIII detector, we present measurements of $J/\psi$ and $\eta^\prime$ absolute branching fractions using the process $J/\psi\rightarrow\gamma\eta^\prime$. By analyzing events where the radiative photon converts into an $e^+e^-$ pair, the branching fraction for $J/\psi \rightarrow \gamma \eta^\prime$ is measured to be $(5.27\pm0.03\pm0.05)\times 10^{-3}$. The absolute branching fractions of the five dominant decay channels of the $\eta^\prime$ are then measured independently for the first time and are determined to be $\mathcal{B}(\eta^\prime \rightarrow \gamma \pi^{+} \pi^{-})$ = (29.90$\pm$0.03$\pm$0.55)%, $\mathcal{B}(\eta^\prime \rightarrow \eta \pi^{+} \pi^{-})$ = (41.24$\pm$0.08$\pm$1.24)%, $\mathcal{B}(\eta^\prime \rightarrow \eta \pi^{0} \pi^{0})$ = (21.36$\pm$0.10$\pm$0.92)%, $\mathcal{B}(\eta^\prime \rightarrow \gamma \omega)$ = (2.489$\pm$0.018$\pm$0.074)%, and $\mathcal{B}(\eta^\prime \rightarrow \gamma \gamma)$ = (2.331$\pm$0.012$\pm$0.035)%, where the first uncertainties are statistical and the second systematic., Comment: 7 pages, 1 figures
Published: 2019
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34. Search for heavy Majorana neutrino in lepton number violating decays of D-> K pi e+ e+

Author: BESIII Collaboration, Ablikim, M., Achasov, M. N., Ahmed, S., Albrecht, M., Alekseev, M., Amoroso, A., An, F. F., An, Q., Bai, J. Z., Bai, Y., Bakina, O., Ferroli, R. Baldini, Ban, Y., Begzsuren, K., Bennett, D. W., Bennett, J. V., Berger, N., Bertani, M., Bettoni, D., Bianchi, F., Boger, E., Boyko, I., Briere, R. A., Cai, H., Cai, X., Cakir, O., Calcaterra, A., Cao, G. F., Cetin, S. A., Chai, J., Chang, J. F., Chelkov, G., Chen, G., Chen, H. S., Chen, J. C., Chen, M. L., Chen, P. L., Chen, S. J., Chen, X. R., Chen, Y. B., Cheng, W., Chu, X. K., Cibinetto, G., Cossio, F., Dai, H. L., Dai, J. P., Dbeyssi, A., Dedovich, D., Deng, Z. Y., Denig, A., Denysenko, I., Destefanis, M., De Mori, F., Ding, Y., Dong, C., Dong, J., Dong, L. Y., Dong, M. Y., Dou, Z. L., Du, S. X., Duan, P. F., Fang, J., Fang, S. S., Fang, Y., Farinelli, R., Fava, L., Fegan, S., Feldbauer, F., Felici, G., Feng, C. Q., Fioravanti, E., Fritsch, M., Fu, C. D., Gao, Q., Gao, X. L., Gao, Y., Gao, Y. G., Gao, Z., Garillon, B., Garzia, I., Gilman, A., Goetzen, K., Gong, L., Gong, W. X., Gradl, W., Greco, M., Gu, M. H., Gu, Y. T., Guo, A. Q., Guo, R. P., Guo, Y. P., Guskov, A., Haddadi, Z., Han, S., Hao, X. Q., Harris, F. A., He, K. L., He, X. Q., Heinsius, F. H., Held, T., Heng, Y. K., Hou, Z. L., Hu, H. M., Hu, J. F., Hu, T., Hu, Y., Huang, G. S., Huang, J. S., Huang, X. T., Huang, X. Z., Huang, Z. L., Hussain, T., Andersson, W. Ikegami, Irshad, M., Ji, Q., Ji, Q. P., Ji, X. B., Ji, X. L., Jiang, X. S., Jiang, X. Y., Jiao, J. B., Jiao, Z., Jin, D. P., Jin, S., Jin, Y., Johansson, T., Julin, A., Kalantar-Nayestanaki, N., Kang, X. S., Kavatsyuk, M., Ke, B. C., Keshk, I. K., Khan, T., Khoukaz, A., Kiese, P., Kiuchi, R., Kliemt, R., Koch, L., Kolcu, O. B., Kopf, B., Kornicer, M., Kuemmel, M., Kuessner, M., Kupsc, A., Kurth, M., Kühn, W., Lange, J. S., Larin, P., Lavezzi, L., Leithoff, H., Li, C., Li, Cheng, Li, D. M., Li, F., Li, F. Y., Li, G., Li, H. B., Li, H. J., Li, J. C., Li, J. W., Li, Jin, Li, K. J., Li, Kang, Li, Ke, Li, Lei, Li, P. L., Li, P. R., Li, Q. Y., Li, W. D., Li, W. G., Li, X. L., Li, X. N., Li, X. Q., Li, Z. B., Liang, H., Liang, Y. F., Liang, Y. T., Liao, G. R., Liao, L. Z., Libby, J., Lin, C. X., Lin, D. X., Liu, B., Liu, B. J., Liu, C. X., Liu, D., Liu, D. Y., Liu, F. H., Liu, Fang, Liu, Feng, Liu, H. B., Liu, H. L, Liu, H. M., Liu, Huanhuan, Liu, Huihui, Liu, J. B., Liu, J. Y., Liu, K., Liu, K. Y., Liu, Ke, Liu, L. D., Liu, Q., Liu, S. B., Liu, X., Liu, Y. B., Liu, Z. A., Liu, Zhiqing, Long, Y. F., Lou, X. C., Lu, H. J., Lu, J. G., Lu, Y., Lu, Y. P., Luo, C. L., Luo, M. X., Luo, T., Luo, X. L., Lusso, S., Lyu, X. R., Ma, F. C., Ma, H. L., Ma, L. L., Ma, M. M., Ma, Q. M., Ma, T., Ma, X. N., Ma, X. Y., Ma, Y. M., Maas, F. E., Maggiora, M., Maldaner, S., Malik, Q. A., Mangoni, A., Mao, Y. J., Mao, Z. P., Marcello, S., Meng, Z. X., Messchendorp, J. G., Mezzadri, G., Min, J., Mitchell, R. E., Mo, X. H., Mo, Y. J., Morales, C. Morales, Muchnoi, N. Yu., Muramatsu, H., Mustafa, A., Nefedov, Y., Nerling, F., Nikolaev, I. B., Ning, Z., Nisar, S., Niu, S. L., Niu, X. Y., Olsen, S. L., Ouyang, Q., Pacetti, S., Pan, Y., Papenbrock, M., Patteri, P., Pelizaeus, M., Pellegrino, J., Peng, H. P., Peng, Z. Y., Peters, K., Pettersson, J., Ping, J. L., Ping, R. G., Pitka, A., Poling, R., Prasad, V., Qi, H. R., Qi, M., Qi, T. . Y., Qian, S., Qiao, C. F., Qin, N., Qin, X. S., Qin, Z. H., Qiu, J. F., Qu, S. Q., Rashid, K. H., Redmer, C. F., Richter, M., Ripka, M., Rivetti, A., Rolo, M., Rong, G., Rosner, Ch., Sarantsev, A., Savrié, M., Schoenning, K., Shan, W., Shan, X. Y., Shao, M., Shen, C. P., Shen, P. X., Shen, X. Y., Sheng, H. Y., Shi, X., Song, J. J., Song, W. M., Song, X. Y., Sosio, S., Sowa, C., Spataro, S., Sun, G. X., Sun, J. F., Sun, L., Sun, S. S., Sun, X. H., Sun, Y. J., Sun, Y. K, Sun, Y. Z., Sun, Z. J., Sun, Z. T., Tan, Y. T, Tang, C. J., Tang, G. Y., Tang, X., Tapan, I., Tiemens, M., Tsednee, B., Uman, I., Wang, B., Wang, B. L., Wang, D., Wang, D. Y., Wang, Dan, Wang, K., Wang, L. L., Wang, L. S., Wang, M., Wang, Meng, Wang, P., Wang, P. L., Wang, W. P., Wang, X. F., Wang, X. L., Wang, Y., Wang, Y. F., Wang, Z., Wang, Z. G., Wang, Z. Y., Wang, Zongyuan, Weber, T., Wei, D. H., Weidenkaff, P., Wen, S. P., Wiedner, U., Wolke, M., Wu, L. H., Wu, L. J., Wu, Z., Xia, L., Xia, Y., Xiao, D., Xiao, Y. J., Xiao, Z. J., Xie, Y. G., Xie, Y. H., Xiong, X. A., Xiu, Q. L., Xu, G. F., Xu, J. J., Xu, L., Xu, Q. J., Xu, Q. N., Xu, X. P., Yan, F., Yan, L., Yan, W. B., Yan, W. C., Yan, Y. H., Yang, H. J., Yang, H. X., Yang, L., Yang, R. X., Yang, Y. H., Yang, Y. X., Yang, Yifan, Yang, Z. Q., Ye, M., Ye, M. H., Yin, J. H., You, Z. Y., Yu, B. X., Yu, C. X., Yu, J. S., Yuan, C. Z., Yuan, Y., Yuncu, A., Zafar, A. A., Zeng, Y., Zhang, B. X., Zhang, B. Y., Zhang, C. C., Zhang, D. H., Zhang, H. H., Zhang, H. Y., Zhang, J., Zhang, J. L., Zhang, J. Q., Zhang, J. W., Zhang, J. Y., Zhang, J. Z., Zhang, K., Zhang, L., Zhang, T. J., Zhang, X. Y., Zhang, Y., Zhang, Y. H., Zhang, Y. T., Zhang, Yang, Zhang, Yao, Zhang, Yi, Zhang, Yu, Zhang, Z. H., Zhang, Z. P., Zhang, Z. Y., Zhao, G., Zhao, J. W., Zhao, J. Y., Zhao, J. Z., Zhao, Lei, Zhao, Ling, Zhao, M. G., Zhao, Q., Zhao, S. J., Zhao, T. C., Zhao, Y. B., Zhao, Z. G., Zhemchugov, A., Zheng, B., Zheng, J. P., Zheng, Y. H., Zhong, B., Zhou, L., Zhou, Q., Zhou, X., Zhou, X. K., Zhou, X. R., Zhou, X. Y., Zhou, Xiaoyu, Zhou, Xu, Zhu, A. N., Zhu, J., Zhu, K., Zhu, K. J., Zhu, S., Zhu, S. H., Zhu, X. L., Zhu, Y. C., Zhu, Y. S., Zhu, Z. A., Zhuang, J., Zou, B. S., and Zou, J. H.
Subjects: High Energy Physics - Experiment
Abstract: Using the data sample of an integrated luminosity of 2.93 fb$^{-1}$ taken at the center-of-mass energy of 3.773 GeV, we search for the Majorana neutrino in the lepton number violating decays $D\to K \pi e^+ e^+$. No significant signal is observed, and the upper limits on the branching fraction at the 90\% confidence level are set to be $\mathcal{B}\,(D^0 \to K^- \pi^- e^+ e^+)<2.8\times10^{-6}$, $\mathcal{B}\,(D^+ \to K_S^0 \pi^- e^+ e^+)<3.3\times10^{-6}$ and $\mathcal{B}\,(D^+ \to K^- \pi^0 e^+ e^+)<8.5\times10^{-6}$. The Majorana neutrino is searched for with different mass assumptions ranging from 0.25 to 1.0 GeV/$c^2$ in the decays $D^0\to K^- e^+ \nu_N(\pi^- e^+)$ and $D^+\to K_S^0 e^+ \nu_N(\pi^- e^+)$, and the upper limits on the branching fraction at the 90\% confidence level are extracted to be at the level of $10^{-7} \sim 10^{-6}$, depending on the mass of Majorana neutrino. The constraints on the mixing matrix element $|V_{eN}|^2$ are also evaluated., Comment: 9 pages,3 figures
Published: 2019
Full Text: View/download PDF

35. Search for rare decay $J/ \psi \to \phi e^+ e^-$

Author: BESIII Collaboration, Ablikim, M., Achasov, M. N., Ahmed, S., Albrecht, M., Alekseev, M., Amoroso, A., An, F. F., An, Q., Bai, Y., Bakina, O., Ferroli, R. Baldini, Ban, Y., Begzsuren, K., Bennett, D. W., Bennett, J. V., Berger, N., Bertani, M., Bettoni, D., Bianchi, F., Boger, E., Boyko, I., Briere, R. A., Cai, H., Cai, X., Calcaterra, A., Cao, G. F., Cetin, S. A., Chai, J., Chang, J. F., Chang, W. L., Chelkov, G., Chen, G., Chen, H. S., Chen, J. C., Chen, M. L., Chen, P. L., Chen, S. J., Chen, X. R., Chen, Y. B., Cheng, W., Chu, X. K., Cibinetto, G., Cossio, F., Dai, H. L., Dai, J. P., Dbeyssi, A., Dedovich, D., Deng, Z. Y., Denig, A., Denysenko, I., Destefanis, M., De Mori, F., Ding, Y., Dong, C., Dong, J., Dong, L. Y., Dong, M. Y., Dou, Z. L., Du, S. X., Duan, P. F., Fang, J., Fang, S. S., Fang, Y., Farinelli, R., Fava, L., Fegan, S., Feldbauer, F., Felici, G., Feng, C. Q., Fioravanti, E., Fritsch, M., Fu, C. D., Gao, Q., Gao, X. L., Gao, Y., Gao, Y. G., Gao, Z., Garillon, B., Garzia, I., Gilman, A., Goetzen, K., Gong, L., Gong, W. X., Gradl, W., Greco, M., Gu, L. M., Gu, M. H., Gu, Y. T., Guo, A. Q., Guo, L. B., Guo, R. P., Guo, Y. P., Guskov, A., Haddadi, Z., Han, S., Hao, X. Q., Harris, F. A., He, K. L., He, X. Q., Heinsius, F. H., Held, T., Heng, Y. K., Hou, Z. L., Hu, H. M., Hu, J. F., Hu, T., Hu, Y., Huang, G. S., Huang, J. S., Huang, X. T., Huang, X. Z., Huang, Z. L., Hussain, T., Andersson, W. Ikegami, Irshad, M., Ji, Q., Ji, Q. P., Ji, X. B., Ji, X. L., Jiang, H. L., Jiang, X. S., Jiang, X. Y., Jiao, J. B., Jiao, Z., Jin, D. P., Jin, S., Jin, Y., Johansson, T., Julin, A., Kalantar-Nayestanaki, N., Kang, X. S., Kavatsyuk, M., Ke, B. C., Keshk, I. K., Khan, T., Khoukaz, A., Kiese, P., Kiuchi, R., Kliemt, R., Koch, L., Kolcu, O. B., Kopf, B., Kornicer, M., Kuemmel, M., Kuessner, M., Kupsc, A., Kurth, M., Kühn, W., Lange, J. S., Larin, P., Lavezzi, L., Leiber, S., Leithoff, H., Li, C., Li, Cheng, Li, D. M., Li, F., Li, F. Y., Li, G., Li, H. B., Li, H. J., Li, J. C., Li, J. W., Li, K. J., Li, Kang, Li, Ke, Li, Lei, Li, P. L., Li, P. R., Li, Q. Y., Li, T., Li, W. D., Li, W. G., Li, X. L., Li, X. N., Li, X. Q., Li, Z. B., Liang, H., Liang, Y. F., Liang, Y. T., Liao, G. R., Liao, L. Z., Libby, J., Lin, C. X., Lin, D. X., Liu, B., Liu, B. J., Liu, C. X., Liu, D., Liu, D. Y., Liu, F. H., Liu, Fang, Liu, Feng, Liu, H. B., Liu, H. L, Liu, H. M., Liu, Huanhuan, Liu, Huihui, Liu, J. B., Liu, J. Y., Liu, K. Y., Liu, Ke, Liu, L. D., Liu, Q., Liu, S. B., Liu, X., Liu, Y. B., Liu, Z. A., Liu, Zhiqing, Long, Y. F., Lou, X. C., Lu, H. J., Lu, J. G., Lu, Y., Lu, Y. P., Luo, C. L., Luo, M. X., Luo, T., Luo, X. L., Lusso, S., Lyu, X. R., Ma, F. C., Ma, H. L., Ma, L. L., Ma, M. M., Ma, Q. M., Ma, X. N., Ma, X. Y., Ma, Y. M., Maas, F. E., Maggiora, M., Maldaner, S., Malik, Q. A., Mangoni, A., Mao, Y. J., Mao, Z. P., Marcello, S., Meng, Z. X., Messchendorp, J. G., Mezzadri, G., Min, J., Min, T. J., Mitchell, R. E., Mo, X. H., Mo, Y. J., Morales, C. Morales, Muchnoi, N. Yu., Muramatsu, H., Mustafa, A., Nakhoul, S., Nefedov, Y., Nerling, F., Nikolaev, I. B., Ning, Z., Nisar, S., Niu, S. L., Niu, X. Y., Olsen, S. L., Ouyang, Q., Pacetti, S., Pan, Y., Papenbrock, M., Patteri, P., Pelizaeus, M., Pellegrino, J., Peng, H. P., Peng, Z. Y., Peters, K., Pettersson, J., Ping, J. L., Ping, R. G., Pitka, A., Poling, R., Prasad, V., Qi, H. R., Qi, M., Qi, T. Y., Qian, S., Qiao, C. F., Qin, N., Qin, X. S., Qin, Z. H., Qiu, J. F., Qu, S. Q., Rashid, K. H., Redmer, C. F., Richter, M., Ripka, M., Rivetti, A., Rolo, M., Rong, G., Rosner, Ch., Sarantsev, A., Savrié, M., Schoenning, K., Shan, W., Shan, X. Y., Shao, M., Shen, C. P., Shen, P. X., Shen, X. Y., Sheng, H. Y., Shi, X., Song, J. J., Song, W. M., Song, X. Y., Sosio, S., Sowa, C., Spataro, S., Sui, F. F., Sun, G. X., Sun, J. F., Sun, L., Sun, S. S., Sun, X. H., Sun, Y. J., Sun, Y. K, Sun, Y. Z., Sun, Z. J., Sun, Z. T., Tan, Y. T, Tang, C. J., Tang, G. Y., Tang, X., Tiemens, M., Tsednee, B., Uman, I., Wang, B., Wang, B. L., Wang, C. W., Wang, D., Wang, D. Y., Wang, Dan, Wang, H. H., Wang, K., Wang, L. L., Wang, L. S., Wang, M., Wang, Meng, Wang, P., Wang, P. L., Wang, W. P., Wang, X. F., Wang, Y., Wang, Y. F., Wang, Z., Wang, Z. G., Wang, Z. Y., Wang, Zongyuan, Weber, T., Wei, D. H., Weidenkaff, P., Wen, S. P., Wiedner, U., Wolke, M., Wu, L. H., Wu, L. J., Wu, Z., Xia, L., Xia, X., Xia, Y., Xiao, D., Xiao, Y. J., Xiao, Z. J., Xie, Y. G., Xie, Y. H., Xiong, X. A., Xiu, Q. L., Xu, G. F., Xu, J. J., Xu, L., Xu, Q. J., Xu, X. P., Yan, F., Yan, L., Yan, W. B., Yan, W. C., Yan, Y. H., Yang, H. J., Yang, H. X., Yang, L., Yang, R. X., Yang, S. L., Yang, Y. H., Yang, Y. X., Yang, Yifan, Yang, Z. Q., Ye, M., Ye, M. H., Yin, J. H., You, Z. Y., Yu, B. X., Yu, C. X., Yu, J. S., Yuan, C. Z., Yuan, Y., Yuncu, A., Zafar, A. A., Zeng, Y., Zhang, B. X., Zhang, B. Y., Zhang, C. C., Zhang, D. H., Zhang, H. H., Zhang, H. Y., Zhang, J., Zhang, J. L., Zhang, J. Q., Zhang, J. W., Zhang, J. Y., Zhang, J. Z., Zhang, K., Zhang, L., Zhang, S. F., Zhang, T. J., Zhang, X. Y., Zhang, Y., Zhang, Y. H., Zhang, Y. T., Zhang, Yang, Zhang, Yao, Zhang, Yu, Zhang, Z. H., Zhang, Z. P., Zhang, Z. Y., Zhao, G., Zhao, J. W., Zhao, J. Y., Zhao, J. Z., Zhao, Lei, Zhao, Ling, Zhao, M. G., Zhao, Q., Zhao, S. J., Zhao, T. C., Zhao, Y. B., Zhao, Z. G., Zhemchugov, A., Zheng, B., Zheng, J. P., Zheng, W. J., Zheng, Y. H., Zhong, B., Zhou, L., Zhou, Q., Zhou, X., Zhou, X. K., Zhou, X. R., Zhou, X. Y., Zhou, Xiaoyu, Zhou, Xu, Zhu, A. N., Zhu, J., Zhu, K., Zhu, K. J., Zhu, S., Zhu, S. H., Zhu, X. L., Zhu, Y. C., Zhu, Y. S., Zhu, Z. A., Zhuang, J., Zou, B. S., and Zou, J. H.
Subjects: High Energy Physics - Experiment
Abstract: Using a data sample of $448.1\times10^6$ $\psi(3686)$ events collected at $\sqrt{s}=$ 3.686 GeV with the BESIII detector at the BEPCII, we search for the rare decay $J/\psi \to \phi e^+ e^-$ via $\psi(3686) \to \pi^+\pi^- J/\psi $. No signal events are observed and the upper limit on the branching fraction is set to be $\mathcal{B}(J/\psi \to \phi e^+ e^-) < 1.2 \times 10^{-7}$ at the 90\% confidence level, which is still about one order of magnitude higher than the Standard Model prediction., Comment: 7 pages, 3 figures
Published: 2019
Full Text: View/download PDF

36. Observation of $\chi_{cJ}\to4K_{S}^{0}$

Author: Ablikim, M., Achasov, M. N., Ahmed, S., Albrecht, M., Alekseev, M., Amoroso, A., An, F. F., An, Q., Bai, Y., Bakina, O., Ferroli, R. Baldini, Ban, Y., Begzsuren, K., Bennett, D. W., Bennett, J. V., Berger, N., Bertani, M., Bettoni, D., Bianchi, F., Boger, E., Boyko, I., Briere, R. A., Cai, H., Cai, X., Calcaterra, A., Cao, G. F., Cetin, S. A., Chai, J., Chang, J. F., Chang, W. L., Chelkov, G., Chen, G., Chen, H. S., Chen, J. C., Chen, M. L., Chen, P. L., Chen, S. J., Chen, X. R., Chen, Y. B., Cheng, W., Chu, X. K., Cibinetto, G., Cossio, F., Dai, H. L., Dai, J. P., Dbeyssi, A., Dedovich, D., Deng, Z. Y., Denig, A., Denysenko, I., Destefanis, M., De Mori, F., Ding, Y., Dong, C., Dong, J., Dong, L. Y., Dong, M. Y., Dou, Z. L., Du, S. X., Duan, P. F., Fang, J., Fang, S. S., Fang, Y., Farinelli, R., Fava, L., Fegan, S., Feldbauer, F., Felici, G., Feng, C. Q., Fritsch, M., Fu, C. D., Gao, Q., Gao, X. L., Gao, Y., Gao, Y. G., Gao, Z., Garillon, B., Garzia, I., Gilman, A., Goetzen, K., Gong, L., Gong, W. X., Gradl, W., Greco, M., Gu, L. M., Gu, M. H., Gu, Y. T., Guo, A. Q., Guo, L. B., Guo, R. P., Guo, Y. P., Guskov, A., Haddadi, Z., Han, S., Hao, X. Q., Harris, F. A., He, K. L., He, X. Q., Heinsius, F. H., Held, T., Heng, Y. K., Hou, Z. L., Hu, H. M., Hu, J. F., Hu, T., Hu, Y., Huang, G. S., Huang, J. S., Huang, X. T., Huang, X. Z., Huang, Z. L., Hussain, T., Andersson, W. Ikegami, Irshad, M., Ji, Q., Ji, Q. P., Ji, X. B., Ji, X. L., Jiang, H. L., Jiang, X. S., Jiang, X. Y., Jiao, J. B., Jiao, Z., Jin, D. P., Jin, S., Jin, Y., Johansson, T., Julin, A., Kalantar-Nayestanaki, N., Kang, X. S., Kavatsyuk, M., Ke, B. C., Keshk, I. K., Khan, T., Khoukaz, A., Kiese, P., Kiuchi, R., Kliemt, R., Koch, L., Kolcu, O. B., Kopf, B., Kornicer, M., Kuemmel, M., Kuessner, M., Kupsc, A., Kurth, M., Kühn, W., Lange, J. S., Larin, P., Lavezzi, L., Leiber, S., Leithoff, H., Li, C., Li, Cheng, Li, D. M., Li, F., Li, F. Y., Li, G., Li, H. B., Li, H. J., Li, J. C., Li, J. W., Li, K. J., Li, Kang, Li, Ke, Li, Lei, Li, P. L., Li, P. R., Li, Q. Y., Li, T., Li, W. D., Li, W. G., Li, X. L., Li, X. N., Li, X. Q., Li, Z. B., Liang, H., Liang, Y. F., Liang, Y. T., Liao, G. R., Liao, L. Z., Libby, J., Lin, C. X., Lin, D. X., Liu, B., Liu, B. J., Liu, C. X., Liu, D., Liu, D. Y., Liu, F. H., Liu, Fang, Liu, Feng, Liu, H. B., Liu, H. L, Liu, H. M., Liu, Huanhuan, Liu, Huihui, Liu, J. B., Liu, J. Y., Liu, K. Y., Liu, Ke, Liu, L. D., Liu, Q., Liu, S. B., Liu, X., Liu, Y. B., Liu, Z. A., Liu, Zhiqing, Long, Y. F., Lou, X. C., Lu, H. J., Lu, J. G., Lu, Y., Lu, Y. P., Luo, C. L., Luo, M. X., Luo, P. W., Luo, T., Luo, X. L., Lusso, S., Lyu, X. R., Ma, F. C., Ma, H. L., Ma, L. L., Ma, M. M., Ma, Q. M., Ma, X. N., Ma, X. Y., Ma, Y. M., Maas, F. E., Maggiora, M., Maldaner, S., Malik, Q. A., Mangoni, A., Mao, Y. J., Mao, Z. P., Marcello, S., Meng, Z. X., Messchendorp, J. G., Mezzadri, G., Min, J., Min, T. J., Mitchell, R. E., Mo, X. H., Mo, Y. J., Morales, C. Morales, Muchnoi, N. Yu., Muramatsu, H., Mustafa, A., Nakhoul, S., Nefedov, Y., Nerling, F., Nikolaev, I. B., Ning, Z., Nisar, S., Niu, S. L., Niu, X. Y., Olsen, S. L., Ouyang, Q., Pacetti, S., Pan, Y., Papenbrock, M., Patteri, P., Pelizaeus, M., Pellegrino, J., Peng, H. P., Peng, Z. Y., Peters, K., Pettersson, J., Ping, J. L., Ping, R. G., Pitka, A., Poling, R., Prasad, V., Qi, H. R., Qi, M., Qi, T. Y., Qian, S., Qiao, C. F., Qin, N., Qin, X. S., Qin, Z. H., Qiu, J. F., Qu, S. Q., Rashid, K. H., Redmer, C. F., Richter, M., Ripka, M., Rivetti, A., Rolo, M., Rong, G., Rosner, Ch., Sarantsev, A., Savrié, M., Schoenning, K., Shan, W., Shan, X. Y., Shao, M., Shen, C. P., Shen, P. X., Shen, X. Y., Sheng, H. Y., Shi, X., Song, J. J., Song, W. M., Song, X. Y., Sosio, S., Sowa, C., Spataro, S., Sui, F. F., Sun, G. X., Sun, J. F., Sun, L., Sun, S. S., Sun, X. H., Sun, Y. J., Sun, Y. K, Sun, Y. Z., Sun, Z. J., Sun, Z. T., Tan, Y. T, Tang, C. J., Tang, G. Y., Tang, X., Tiemens, M., Tsednee, B., Uman, I., Wang, B., Wang, B. L., Wang, C. W., Wang, D., Wang, D. Y., Wang, Dan, Wang, H. H., Wang, K., Wang, L. L., Wang, L. S., Wang, M., Wang, Meng, Wang, P., Wang, P. L., Wang, W. P., Wang, X. F., Wang, Y., Wang, Y. F., Wang, Z., Wang, Z. G., Wang, Z. Y., Wang, Zongyuan, Weber, T., Wei, D. H., Weidenkaff, P., Wen, S. P., Wiedner, U., Wolke, M., Wu, L. H., Wu, L. J., Wu, Z., Xia, L., Xia, X., Xia, Y., Xiao, D., Xiao, Y. J., Xiao, Z. J., Xie, Y. G., Xie, Y. H., Xiong, X. A., Xiu, Q. L., Xu, G. F., Xu, J. J., Xu, L., Xu, Q. J., Xu, X. P., Yan, F., Yan, L., Yan, W. B., Yan, W. C., Yan, Y. H., Yang, H. J., Yang, H. X., Yang, L., Yang, R. X., Yang, S. L., Yang, Y. H., Yang, Y. X., Yang, Yifan, Yang, Z. Q., Ye, M., Ye, M. H., Yin, J. H., You, Z. Y., Yu, B. X., Yu, C. X., Yu, J. S., Yuan, C. Z., Yuan, Y., Yuncu, A., Zafar, A. A., Zeng, Y., Zhang, B. X., Zhang, B. Y., Zhang, C. C., Zhang, D. H., Zhang, H. H., Zhang, H. Y., Zhang, J., Zhang, J. L., Zhang, J. Q., Zhang, J. W., Zhang, J. Y., Zhang, J. Z., Zhang, K., Zhang, L., Zhang, S. F., Zhang, T. J., Zhang, X. Y., Zhang, Y., Zhang, Y. H., Zhang, Y. T., Zhang, Yang, Zhang, Yao, Zhang, Yu, Zhang, Z. H., Zhang, Z. P., Zhang, Z. Y., Zhao, G., Zhao, J. W., Zhao, J. Y., Zhao, J. Z., Zhao, Lei, Zhao, Ling, Zhao, M. G., Zhao, Q., Zhao, S. J., Zhao, T. C., Zhao, Y. B., Zhao, Z. G., Zhemchugov, A., Zheng, B., Zheng, J. P., Zheng, W. J., Zheng, Y. H., Zhong, B., Zhou, L., Zhou, Q., Zhou, X., Zhou, X. K., Zhou, X. R., Zhou, X. Y., Zhou, Xiaoyu, Zhou, Xu, Zhu, A. N., Zhu, J., Zhu, K., Zhu, K. J., Zhu, S., Zhu, S. H., Zhu, X. L., Zhu, Y. C., Zhu, Y. S., Zhu, Z. A., Zhuang, J., Zou, B. S., and Zou, J. H.
Subjects: High Energy Physics - Experiment
Abstract: By analyzing $(448.1\pm2.9)\times10^6$ $\psi(3686)$ events collected with the BESIII detector operating at the BEPCII collider, the decays of $\chi_{cJ} \to 4K_S^0$ ($J=0,1,2$) are observed for the first time with statistical significances of 26.5$\sigma$, 5.9$\sigma$ and 11.4$\sigma$, respectively. The product branching fractions of $\psi(3686)\to\gamma\chi_{cJ}$, $\chi_{cJ}\to4K_{S}^{0}$ are presented and the branching fractions of $\chi_{cJ}\to4K_{S}^{0}$ decays are determined to be $\mathcal{B}_{\chi_{c0}\to 4K_S^0}$=$(5.76\pm0.34\pm0.38)$$\times10^{-4}$, $\mathcal{B}_{\chi_{c1}\to 4K_S^0}$=$(0.35\pm0.09\pm0.03)$$\times10^{-4}$ and $\mathcal{B}_{\chi_{c2}\to 4K_S^0}$=$(1.14\pm0.15\pm0.08)$$\times10^{-4}$, where the first uncertainties are statistical and the second are systematic, respectively.
Published: 2019
Full Text: View/download PDF

37. Study of electromagnetic Dalitz decays $\chi_{cJ} \rightarrow \mu^{+}\mu^{-}J/\psi$

Author: Ablikim, M., Achasov, M. N., Ahmed, S., Albrecht, M., Alekseev, M., Amoroso, A., An, F. F., An, Q., Bai, Y., Bakina, O., Ferroli, R. Baldini, Ban, Y., Begzsuren, K., Bennett, D. W., Bennett, J. V., Berger, N., Bertani, M., Bettoni, D., Bianchi, F., Bloms, J., Boyko, I., Briere, R. A., Cai, H., Cai, X., Calcaterra, A., Cao, G. F., Cetin, S. A., Chai, J., Chang, J. F., Chang, W. L., Chelkov, G., Chen, G., Chen, H. S., Chen, J. C., Chen, M. L., Chen, S. J., Chen, Y. B., Cheng, W., Cibinetto, G., Cossio, F., Dai, H. L., Dai, J. P., Dbeyssi, A., Dedovich, D., Deng, Z. Y., Denig, A., Denysenko, I., Destefanis, M., De Mori, F., Ding, Y., Dong, C., Dong, J., Dong, L. Y., Dong, M. Y., Dou, Z. L., Du, S. X., Fan, J. Z., Fang, J., Fang, S. S., Fang, Y., Farinelli, R., Fava, L., Feldbauer, F., Felici, G., Feng, C. Q., Fritsch, M., Fu, C. D., Fu, Y., Gao, Q., Gao, X. L., Gao, Y., Gao, Y. G., Gao, Z., Garillon, B., Garzia, I., Gilman, A., Goetzen, K., Gong, L., Gong, W. X., Gradl, W., Greco, M., Gu, L. M., Gu, M. H., Gu, Y. T., Guo, A. Q., Guo, L. B., Guo, R. P., Guo, Y. P., Guskov, A., Han, S., Hao, X. Q., Harris, F. A., He, K. L., Heinsius, F. H., Held, T., Heng, Y. K., Hou, Z. L., Hu, H. M., Hu, J. F., Hu, T., Hu, Y., Huang, G. S., Huang, J. S., Huang, X. T., Huang, X. Z., Huang, Z. L., Hussain, T., Hsken, N., Andersson, W. Ikegami, Imoehl, W., Irshad, M., Ji, Q., Ji, Q. P., Ji, X. B., Ji, X. L., Jiang, H. L., Jiang, X. S., Jiang, X. Y., Jiao, J. B., Jiao, Z., Jin, D. P., Jin, S., Jin, Y., Johansson, T., Kalantar-Nayestanaki, N., Kang, X. S., Kavatsyuk, M., Ke, B. C., Keshk, I. K., Khan, T., Khoukaz, A., Kiese, P., Kiuchi, R., Kliemt, R., Koch, L., Kolcu, O. B., Kopf, B., Kuemmel, M., Kuessner, M., Kupsc, A., Kurth, M., Kühn, W., Lange, J. S., Larin, P., Lavezzi, L., Leithoff, H., Li, C., Li, Cheng, Li, D. M., Li, F., Li, F. Y., Li, G., Li, H. B., Li, H. J., Li, J. C., Li, J. W., Li, Ke, Li, L. K., Li, Lei, Li, P. L., Li, P. R., Li, Q. Y., Li, W. D., Li, W. G., Li, X. L., Li, X. N., Li, X. Q., Li, X. H., Li, Z. B., Liang, H., Liang, Y. F., Liang, Y. T., Liao, G. R., Liao, L. Z., Libby, J., Lin, C. X., Lin, D. X., Liu, B., Liu, B. J., Liu, C. X., Liu, D., Liu, D. Y., Liu, F. H., Liu, Fang, Liu, Feng, Liu, H. B., Liu, H. L, Liu, H. M., Liu, Huanhuan, Liu, Huihui, Liu, J. B., Liu, J. Y., Liu, K. Y., Liu, Ke, Liu, Q., Liu, S. B., Liu, X., Liu, Y. B., Liu, Z. A., Liu, Zhiqing, Long, Y. F., Lou, X. C., Lu, H. J., Lu, J. D., Lu, J. G., Lu, Y., Lu, Y. P., Luo, C. L., Luo, M. X., Luo, P. W., Luo, T., Luo, X. L., Lusso, S., Lyu, X. R., Ma, F. C., Ma, H. L., Ma, L. L., Ma, M. M., Ma, Q. M., Ma, X. N., Ma, X. X., Ma, X. Y., Ma, Y. M., Maas, F. E., Maggiora, M., Maldaner, S., Malik, Q. A., Mangoni, A., Mao, Y. J., Mao, Z. P., Marcello, S., Meng, Z. X., Messchendorp, J. G., Mezzadri, G., Min, J., Min, T. J., Mitchell, R. E., Mo, X. H., Mo, Y. J., Morales, C. Morales, Muchnoi, N. Yu., Muramatsu, H., Mustafa, A., Nakhoul, S., Nefedov, Y., Nerling, F., Nikolaev, I. B., Ning, Z., Nisar, S., Niu, S. L., Olsen, S. L., Ouyang, Q., Pacetti, S., Pan, Y., Papenbrock, M., Patteri, P., Pelizaeus, M., Peng, H. P., Peters, K., Pettersson, J., Ping, J. L., Ping, R. G., Pitka, A., Poling, R., Prasad, V., Qi, M., Qi, T. Y., Qian, S., Qiao, C. F., Qin, N., Qin, X. S., Qin, Z. H., Qiu, J. F., Qu, S. Q., Rashid, K. H., Redmer, C. F., Richter, M., Ripka, M., Rivetti, A., Rolo, M., Rong, G., Rosner, Ch., Rump, M., Sarantsev, A., Savrié, M., Schoenning, K., Shan, W., Shan, X. Y., Shao, M., Shen, C. P., Shen, P. X., Shen, X. Y., Sheng, H. Y., Shi, X., Shi, X. D, Song, J. J., Song, Q. Q., Song, X. Y., Sosio, S., Sowa, C., Spataro, S., Sui, F. F., Sun, G. X., Sun, J. F., Sun, L., Sun, S. S., Sun, X. H., Sun, Y. J., Sun, Y. K, Sun, Y. Z., Sun, Z. J., Sun, Z. T., Tan, Y. T, Tang, C. J., Tang, G. Y., Tang, X., Tsednee, B., Uman, I., Wang, B., Wang, B. L., Wang, C. W., Wang, D. Y., Wang, H. H., Wang, K., Wang, L. L., Wang, L. S ., Wang, M., Wang, M. Z., Wang, Meng, Wang, P., Wang, P. L., Wang, R. M., Wang, W. P., Wang, X., Wang, X. F., Wang, Y., Wang, Y. F., Wang, Z., Wang, Z. G., Wang, Z. Y., Wang, Zongyuan, Weber, T., Wei, D. H., Weidenkaff, P., Wen, S. P., Wiedner, U., Wolke, M., Wu, L. H., Wu, L. J., Wu, Z., Xia, L., Xia, Y., Xiao, Y. J., Xiao, Z. J., Xie, Y. G., Xie, Y. H., Xiong, X. A., Xiu, Q. L., Xu, G. F., Xu, L., Xu, Q . J., Xu, W., Xu, X. P., Yan, F., Yan, L., Yan, W. B., Yan, W. C., Yan, Y. H., Yang, H. J., Yang, H. X., Yang, L., Yang, R. X., Yang, S. L., Yang, Y. H., Yang, Y. X., Yang, Yifan, Yang, Z. Q., Ye, M., Ye, M. H., Yin, J. H., You, Z. Y., Yu, B. X., Yu, C. X., Yu, J. S., Yuan, C . Z., Yuan, Y., Yuncu, A., Zafar, A. A., Zeng, Y., Zhang, B. X., Zhang, B. Y., Zhang, C. C., Zhang, D. H., Zhang, H. H., ang, H. Y. Zh, Zhang, J., Zhang, J. L., Zhang, J. Q., Zhang, J. W., Zhang, J. Y., Zhang, J. Z., Zhang, K., Zhang, L., Zhang, S. F., Zhang, T. J., Zhang, X. Y., Zhang, Y., Zhang, Y. H., Zhang, Y. T., Zhang, Yang, Zhang, Yao, Zhang, Yu, Zhang, Z. H., Zhang, Z. P., Zhang, Z. Y., Zhao, G., Zhao, J. W., Zhao, J. Y., Zhao, J. Z., Zhao, Lei, Zhao, Ling, Zhao, M. G., Zhao, Q., Zhao, S. J., Zhao, T. C., Zhao, Y. B., Zhao, Z. G., Zhemchugov, A., Zheng, B., Zheng, J. P., Zheng, Y., Zheng, Y. H., Zhong, B., Zhou, L., Zhou, Q., Zhou, X., Zhou, X. K., ou, X. R. Zh, Zhou, Xiaoyu, Zhou, Xu, Zhu, A. N., Zhu, J., Zhu, K., Zhu, K. J., Zhu, S. H., Zhu, X. L., Zhu, Y. C., Zhu, Y. S., u, Z. A. Zh, Zhuang, J., Zou, B. S., and Zou, J. H.
Subjects: High Energy Physics - Experiment
Abstract: Using $4.48 \times 10^{8}$ $\psi(3686)$ events collected with the BESIII detector, we search for the decays $\chi_{cJ} \rightarrow \mu^{+}\mu^{-}J/\psi$ through the radiative decays $\psi(3686) \rightarrow \gamma\chi_{cJ}$, where $J=0,1,2$. The decays $\chi_{c1,2} \rightarrow \mu^{+}\mu^{-}J/\psi$ are observed, and the corresponding branching fractions are measured to be $\mathcal{B}(\chi_{c1} \rightarrow \mu^{+}\mu^{-}J/\psi) = (2.51 \pm 0.18 \pm 0.20)\times10^{-4}$ and $\mathcal{B}(\chi_{c2} \rightarrow \mu^{+}\mu^{-}J/\psi) = (2.33 \pm 0.18 \pm 0.29)\times10^{-4}$, where the first uncertainty is statistical and the second one systematic. No significant $\chi_{c0} \rightarrow \mu^{+}\mu^{-}J/\psi$ decay is observed, and the upper limit on the branching fraction is determined to be $2.0\times10^{-5}$ at 90% confidence level. Also, we present a study of di-muon invariant mass dependent transition form factor for the decays $\chi_{c1,2} \rightarrow \mu^{+}\mu^{-}J/\psi$.
Published: 2019
Full Text: View/download PDF

38. Amplitude analysis of $D^{+} \rightarrow K_{S}^{0} \pi^{+} \pi^{+} \pi^{-}$

Author: Ablikim, M., Achasov, M. N., Ahmed, S., Albrecht, M., Alekseev, M., Amoroso, A., An, F. F., An, Q., Bai, J. Z., Bai, Y., Bakina, O., Ferroli, R. Baldini, Ban, Y., Begzsuren, K., Bennett, D. W., Bennett, J. V., Berger, N., Bertani, M., Bettoni, D., Bianchi, F., Boger, E., Boyko, I., Briere, R. A., Cai, H., Cai, X., Calcaterra, A., Cao, G. F., Cetin, S. A., Chai, J., Chang, J. F., Chelkov, G., Chen, G., Chen, H. S., Chen, J. C., Chen, M. L., Chen, P. L., Chen, S. J., Chen, X. R., Chen, Y. B., Cheng, W., Chu, X. K., Cibinetto, G., Cossio, F., Dai, H. L., Dai, J. P., Dbeyssi, A., Dedovich, D., Deng, Z. Y., Denig, A., Denysenko, I., Destefanis, M., De Mori, F., Ding, Y., Dong, C., Dong, J., Dong, L. Y., Dong, M. Y., Dou, Z. L., Du, S. X., Duan, P. F., Fang, J., Fang, S. S., Fang, Y., Farinelli, R., Fava, L., Fegan, S., Feldbauer, F., Felici, G., Feng, C. Q., Fioravanti, E., Fritsch, M., Fu, C. D., Gao, Q., Gao, X. L., Gao, Y., Gao, Y. G., Gao, Z., Garillon, B., Garzia, I., Gilman, A., Goetzen, K., Gong, L., Gong, W. X., Gradl, W., Greco, M., Gu, L. M., Gu, M. H., Gu, Y. T., Guo, A. Q., Guo, L. B., Guo, R. P., Guo, Y. P., Guskov, A., Haddadi, Z., Han, S., Hao, X. Q., Harris, F. A., He, K. L., He, X. Q., Heinsius, F. H., Held, T., Heng, Y. K., Hou, Z. L., Hu, H. M., Hu, J. F., Hu, T., Hu, Y., Huang, G. S., Huang, J. S., Huang, X. T., Huang, X. Z., Huang, Z. L., Hussain, T., Andersson, W. Ikegami, Irshad, M., Ji, Q., Ji, Q. P., Ji, X. B., Ji, X. L., Jiang, X. S., Jiang, X. Y., Jiao, J. B., Jiao, Z., Jin, D. P., Jin, S., Jin, Y., Johansson, T., Julin, A., Kalantar-Nayestanaki, N., Kang, X. S., Kavatsyuk, M., Ke, B. C., Keshk, I. K., Khan, T., Khoukaz, A., Kiese, P., Kiuchi, R., Kliemt, R., Koch, L., Kolcu, O. B., Kopf, B., Kornicer, M., Kuemmel, M., Kuessner, M., Kupsc, A., Kurth, M., Kühn, W., Lange, J. S., Larin, P., Lavezzi, L., Leiber, S., Leithoff, H., Li, C., Li, Cheng, Li, D. M., Li, F., Li, F. Y., Li, G., Li, H. B., Li, H. J., Li, J. C., Li, J. W., Li, K. J., Li, Kang, Li, Ke, Li, Lei, Li, P. L., Li, P. R., Li, Q. Y., Li, T., Li, W. D., Li, W. G., Li, X. L., Li, X. N., Li, X. Q., Li, Z. B., Liang, H., Liang, Y. F., Liang, Y. T., Liao, G. R., Liao, L. Z., Libby, J., Lin, C. X., Lin, D. X., Liu, B., Liu, B. J., Liu, C. X., Liu, D., Liu, D. Y., Liu, F. H., Liu, Fang, Liu, Feng, Liu, H. B., Liu, H. L, Liu, H. M., Liu, Huanhuan, Liu, Huihui, Liu, J. B., Liu, J. Y., Liu, K. Y., Liu, Ke, Liu, L. D., Liu, Q., Liu, S. B., Liu, X., Liu, Y. B., Liu, Z. A., Liu, Zhiqing, Long, Y. F., Lou, X. C., Lu, H. J., Lu, J. G., Lu, Y., Lu, Y. P., Luo, C. L., Luo, M. X., Luo, T., Luo, X. L., Lusso, S., Lyu, X. R., Ma, F. C., Ma, H. L., Ma, L. L., Ma, M. M., Ma, Q. M., Ma, T., Ma, X. N., Ma, X. Y., Ma, Y. M., Maas, F. E., Maggiora, M., Maldaner, S., Malik, Q. A., Mangoni, A., Mao, Y. J., Mao, Z. P., Marcello, S., Meng, Z. X., Messchendorp, J. G., Mezzadri, G., Min, J., Min, T. J., Mitchell, R. E., Mo, X. H., Mo, Y. J., Morales, C. Morales, Muchnoi, N. Yu., Muramatsu, H., Mustafa, A., Nakhoul, S., Nefedov, Y., Nerling, F., Nikolaev, I. B., Ning, Z., Nisar, S., Niu, S. L., Niu, X. Y., Olsen, S. L., Ouyang, Q., Pacetti, S., Pan, Y., Papenbrock, M., Patteri, P., Pelizaeus, M., Pellegrino, J., Peng, H. P., Peng, Z. Y., Peters, K., Pettersson, J., Ping, J. L., Ping, R. G., Pitka, A., Poling, R., Prasad, V., Qi, H. R., Qi, M., Qi, T. Y., Qian, S., Qiao, C. F., Qin, N., Qin, X. S., Qin, Z. H., Qiu, J. F., Qu, S. Q., Rashid, K. H., Redmer, C. F., Richter, M., Ripka, M., Rivetti, A., Rolo, M., Rong, G., Rosner, Ch., Sarantsev, A., Savrié, M., Schoenning, K., Shan, W., Shan, X. Y., Shao, M., Shen, C. P., Shen, P. X., Shen, X. Y., Sheng, H. Y., Shi, X., Song, J. J., Song, W. M., Song, X. Y., Sosio, S., Sowa, C., Spataro, S., Sun, G. X., Sun, J. F., Sun, L., Sun, S. S., Sun, X. H., Sun, Y. J., Sun, Y. K, Sun, Y. Z., Sun, Z. J., Sun, Z. T., Tan, Y. T, Tang, C. J., Tang, G. Y., Tang, X., Tiemens, M., Tsednee, B., Uman, I., Wang, B., Wang, B. L., Wang, C. W., Wang, D., Wang, D. Y., Wang, Dan, Wang, K., Wang, L. L., Wang, L. S., Wang, M., Wang, Meng, Wang, P., Wang, P. L., Wang, W. P., Wang, X. F., Wang, Y., Wang, Y. F., Wang, Z., Wang, Z. G., Wang, Z. Y., Wang, Zongyuan, Weber, T., Wei, D. H., Weidenkaff, P., Wen, S. P., Wiedner, U., Wolke, M., Wu, L. H., Wu, L. J., Wu, Z., Xia, L., Xia, X., Xia, Y., Xiao, D., Xiao, Y. J., Xiao, Z. J., Xie, Y. G., Xie, Y. H., Xiong, X. A., Xiu, Q. L., Xu, G. F., Xu, J. J., Xu, L., Xu, Q. J., Xu, X. P., Yan, F., Yan, L., Yan, W. B., Yan, W. C., Yan, Y. H., Yang, H. J., Yang, H. X., Yang, L., Yang, R. X., Yang, Y. H., Yang, Y. X., Yang, Yifan, Yang, Z. Q., Ye, M., Ye, M. H., Yin, J. H., You, Z. Y., Yu, B. X., Yu, C. X., Yu, J. S., Yuan, C. Z., Yuan, Y., Yuncu, A., Zafar, A. A., Zeng, Y., Zhang, B. X., Zhang, B. Y., Zhang, C. C., Zhang, D. H., Zhang, H. H., Zhang, H. Y., Zhang, J., Zhang, J. L., Zhang, J. Q., Zhang, J. W., Zhang, J. Y., Zhang, J. Z., Zhang, K., Zhang, L., Zhang, S. F., Zhang, T. J., Zhang, X. Y., Zhang, Y., Zhang, Y. H., Zhang, Y. T., Zhang, Yang, Zhang, Yao, Zhang, Yu, Zhang, Z. H., Zhang, Z. P., Zhang, Z. Y., Zhao, G., Zhao, J. W., Zhao, J. Y., Zhao, J. Z., Zhao, Lei, Zhao, Ling, Zhao, M. G., Zhao, Q., Zhao, S. J., Zhao, T. C., Zhao, Y. B., Zhao, Z. G., Zhemchugov, A., Zheng, B., Zheng, J. P., Zheng, W. J., Zheng, Y. H., Zhong, B., Zhou, L., Zhou, Q., Zhou, X., Zhou, X. K., Zhou, X. R., Zhou, X. Y., Zhou, Xiaoyu, Zhou, Xu, Zhu, A. N., Zhu, J., Zhu, K., Zhu, K. J., Zhu, S., Zhu, S. H., Zhu, X. L., Zhu, Y. C., Zhu, Y. S., Zhu, Z. A., Zhuang, J., Zou, B. S., and Zou, J. H.
Subjects: High Energy Physics - Experiment
Abstract: The decay $D^{+} \rightarrow K_{S}^{0} \pi^{+} \pi^{+} \pi^{-}$ is studied with an amplitude analysis using a data set of 2.93${\mbox{\,fb}^{-1}}$ of $e^+e^+$ collisions at the $\psi(3770)$ peak accumulated by the BESIII detector. Intermediate states and non-resonant components, and their relative fractions and phases have been determined. The significant amplitudes, which contribute to the model that best fits the data, are composed of five quasi-two-body decays $ K_{S}^{0} a_{1}(1260)^{+}$, $ \bar{K}_{1}(1270)^{0} \pi^{+}$ $ \bar{K}_{1}(1400)^{0} \pi^{+}$, $ \bar{K}_{1}(1650)^{0} \pi^{+}$, and $ \bar{K}(1460)^{0} \pi^{+}$, a three-body decays $K_{S}^{0}\pi^{+}\rho^{0}$, as well as a non-resonant component $ K_{S}^{0}\pi^{+}\pi^{+}\pi^{-}$. The dominant amplitude is $ K_{S}^{0} a_{1}(1260)^{+}$, with a fit fraction of $(40.3\pm2.1\pm2.9)\%$, where the first and second uncertainties are statistical and systematic, respectively., Comment: 14 pages, 3 figures
Published: 2019
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39. Measurement of the Dynamics of the Decays ${ D_s^+ \rightarrow \eta^{(\prime)} e^{+} \nu_e}$

Author: Ablikim, M., Achasov, M. N., Ahmed, S., Albrecht, M., Alekseev, M., Amoroso, A., An, F. F., An, Q., Bai, J. Z., Bai, Y., Bakina, O., Ferroli, R. Baldini, Ban, Y., Begzsuren, K., Bennett, D. W., Bennett, J. V., Berger, N., Bertani, M., Bettoni, D., Bianchi, F., Boger, E., Boyko, I., Briere, R. A., Cai, H., Cai, X., Calcaterra, A., Cao, G. F., Cetin, S. A., Chai, J., Chang, J. F., Chelkov, G., Chen, G., Chen, H. S., Chen, J. C., Chen, M. L., Chen, P. L., Chen, S. J., Chen, X. R., Chen, Y. B., Cheng, W., Chu, X. K., Cibinetto, G., Cossio, F., Dai, H. L., Dai, J. P., Dbeyssi, A., Dedovich, D., Deng, Z. Y., Denig, A., Denysenko, I., Destefanis, M., De Mori, F., Ding, Y., Dong, C., Dong, J., Dong, L. Y., Dong, M. Y., Dou, Z. L., Du, S. X., Duan, P. F., Fang, J., Fang, S. S., Fang, Y., Farinelli, R., Fava, L., Fegan, S., Feldbauer, F., Felici, G., Feng, C. Q., Fioravanti, E., Fritsch, M., Fu, C. D., Gao, Q., Gao, X. L., Gao, Y., Gao, Y. G., Gao, Z., Garillon, B., Garzia, I., Gilman, A., Goetzen, K., Gong, L., Gong, W. X., Gradl, W., Greco, M., Gu, L. M., Gu, M. H., Gu, Y. T., Guo, A. Q., Guo, L. B., Guo, R. P., Guo, Y. P., Guskov, A., Haddadi, Z., Han, S., Hao, X. Q., Harris, F. A., He, K. L., He, X. Q., Heinsius, F. H., Held, T., Heng, Y. K., Hou, Z. L., Hu, H. M., Hu, J. F., Hu, T., Hu, Y., Huang, G. S., Huang, J. S., Huang, X. T., Huang, X. Z., Huang, Z. L., Hussain, T., Andersson, W. Ikegami, Irshad, M., Ji, Q., Ji, Q. P., Ji, X. B., Ji, X. L., Jiang, X. S., Jiang, X. Y., Jiao, J. B., Jiao, Z., Jin, D. P., Jin, S., Jin, Y., Johansson, T., Julin, A., Kalantar-Nayestanaki, N., Kang, X. S., Kavatsyuk, M., Ke, B. C., Keshk, I. K., Khan, T., Khoukaz, A., Kiese, P., Kiuchi, R., Kliemt, R., Koch, L., Kolcu, O. B., Kopf, B., Kornicer, M., Kuemmel, M., Kuessner, M., Kupsc, A., Kurth, M., Kühn, W., Lange, J. S., Larin, P., Lavezzi, L., Leiber, S., Leithoff, H., Li, C., Li, Cheng, Li, D. M., Li, F., Li, F. Y., Li, G., Li, H. B., Li, H. J., Li, J. C., Li, J. W., Li, K. J., Li, Kang, Li, Ke, Li, Lei, Li, P. L., Li, P. R., Li, Q. Y., Li, T., Li, W. D., Li, W. G., Li, X. L., Li, X. N., Li, X. Q., Li, Z. B., Liang, H., Liang, Y. F., Liang, Y. T., Liao, G. R., Liao, L. Z., Libby, J., Lin, C. X., Lin, D. X., Liu, B., Liu, B. J., Liu, C. X., Liu, D., Liu, D. Y., Liu, F. H., Liu, Fang, Liu, Feng, Liu, H. B., Liu, H. L, Liu, H. M., Liu, Huanhuan, Liu, Huihui, Liu, J. B., Liu, J. Y., Liu, K. Y., Liu, Ke, Liu, L. D., Liu, Q., Liu, S. B., Liu, X., Liu, Y. B., Liu, Z. A., Liu, Zhiqing, Long, Y. F., Lou, X. C., Lu, H. J., Lu, J. G., Lu, Y., Lu, Y. P., Luo, C. L., Luo, M. X., Luo, T., Luo, X. L., Lusso, S., Lyu, X. R., Ma, F. C., Ma, H. L., Ma, L. L., Ma, M. M., Ma, Q. M., Ma, T., Ma, X. N., Ma, X. Y., Ma, Y. M., Maas, F. E., Maggiora, M., Maldaner, S., Malik, Q. A., Mangoni, A., Mao, Y. J., Mao, Z. P., Marcello, S., Meng, Z. X., Messchendorp, J. G., Mezzadri, G., Min, J., Min, T. J., Mitchell, R. E., Mo, X. H., Mo, Y. J., Morales, C. Morales, Muchnoi, N. Yu., Muramatsu, H., Mustafa, A., Nakhoul, S., Nefedov, Y., Nerling, F., Nikolaev, I. B., Ning, Z., Nisar, S., Niu, S. L., Niu, X. Y., Olsen, S. L., Ouyang, Q., Pacetti, S., Pan, Y., Papenbrock, M., Patteri, P., Pelizaeus, M., Pellegrino, J., Peng, H. P., Peng, Z. Y., Peters, K., Pettersson, J., Ping, J. L., Ping, R. G., Pitka, A., Poling, R., Prasad, V., Qi, H. R., Qi, M., Qi, T. Y., Qian, S., Qiao, C. F., Qin, N., Qin, X. S., Qin, Z. H., Qiu, J. F., Qu, S. Q., Rashid, K. H., Redmer, C. F., Richter, M., Ripka, M., Rivetti, A., Rolo, M., Rong, G., Rosner, Ch., Sarantsev, A., Savrié, M., Schoenning, K., Shan, W., Shan, X. Y., Shao, M., Shen, C. P., Shen, P. X., Shen, X. Y., Sheng, H. Y., Shi, X., Song, J. J., Song, W. M., Song, X. Y., Sosio, S., Sowa, C., Spataro, S., Sun, G. X., Sun, J. F., Sun, L., Sun, S. S., Sun, X. H., Sun, Y. J., Sun, Y. K, Sun, Y. Z., Sun, Z. J., Sun, Z. T., Tan, Y. T, Tang, C. J., Tang, G. Y., Tang, X., Tiemens, M., Tsednee, B., Uman, I., Wang, B., Wang, B. L., Wang, C. W., Wang, D., Wang, D. Y., Wang, Dan, Wang, K., Wang, L. L., Wang, L. S., Wang, M., Wang, Meng, Wang, P., Wang, P. L., Wang, W. P., Wang, X. F., Wang, Y., Wang, Y. F., Wang, Z., Wang, Z. G., Wang, Z. Y., Wang, Zongyuan, Weber, T., Wei, D. H., Weidenkaff, P., Wen, S. P., Wiedner, U., Wolke, M., Wu, L. H., Wu, L. J., Wu, Z., Xia, L., Xia, X., Xia, Y., Xiao, D., Xiao, Y. J., Xiao, Z. J., Xie, Y. G., Xie, Y. H., Xiong, X. A., Xiu, Q. L., Xu, G. F., Xu, J. J., Xu, L., Xu, Q. J., Xu, X. P., Yan, F., Yan, L., Yan, W. B., Yan, W. C., Yan, Y. H., Yang, H. J., Yang, H. X., Yang, L., Yang, R. X., Yang, Y. H., Yang, Y. X., Yang, Yifan, Yang, Z. Q., Ye, M., Ye, M. H., Yin, J. H., You, Z. Y., Yu, B. X., Yu, C. X., Yu, J. S., Yuan, C. Z., Yuan, Y., Yuncu, A., Zafar, A. A., Zeng, Y., Zhang, B. X., Zhang, B. Y., Zhang, C. C., Zhang, D. H., Zhang, H. H., Zhang, H. Y., Zhang, J., Zhang, J. L., Zhang, J. Q., Zhang, J. W., Zhang, J. Y., Zhang, J. Z., Zhang, K., Zhang, L., Zhang, S. F., Zhang, T. J., Zhang, X. Y., Zhang, Y., Zhang, Y. H., Zhang, Y. T., Zhang, Yang, Zhang, Yao, Zhang, Yu, Zhang, Z. H., Zhang, Z. P., Zhang, Z. Y., Zhao, G., Zhao, J. W., Zhao, J. Y., Zhao, J. Z., Zhao, Lei, Zhao, Ling, Zhao, M. G., Zhao, Q., Zhao, S. J., Zhao, T. C., Zhao, Y. B., Zhao, Z. G., Zhemchugov, A., Zheng, B., Zheng, J. P., Zheng, W. J., Zheng, Y. H., Zhong, B., Zhou, L., Zhou, Q., Zhou, X., Zhou, X. K., Zhou, X. R., Zhou, X. Y., Zhou, Xiaoyu, Zhou, Xu, Zhu, A. N., Zhu, J., Zhu, K., Zhu, K. J., Zhu, S., Zhu, S. H., Zhu, X. L., Zhu, Y. C., Zhu, Y. S., Zhu, Z. A., Zhuang, J., Zou, B. S., and Zou, J. H.
Subjects: High Energy Physics - Experiment
Abstract: Using $e^+e^-$ annihilation data corresponding to an integrated luminosity of 3.19\,fb$^{-1}$ collected at a center-of-mass energy of 4.178~GeV with the BESIII detector, we measure the absolute branching fractions $\mathcal{B}_{D_s^+ \rightarrow \eta e^{+} \nu_e }$ = $(2.323\pm0.063_{\rm stat}\pm0.063_{\rm syst})\%$ and $\mathcal{B}_{D_s^+ \rightarrow \eta^{\prime} e^{+} \nu_e}$ = $(0.824\pm0.073_{\rm stat}\pm0.027_{\rm syst})\%$ via a tagged analysis technique, where one $D_s$ is fully reconstructed in a hadronic mode. Combining these measurements with previous BESIII measurements of $\mathcal{B}_{D^+\to\eta^{(\prime)} e^{+} \nu_e}$, the $\eta-\eta^\prime$ mixing angle in the quark flavour basis is determined to be $\phi_{\rm P} = (40.1\pm2.1_{\rm stat}\pm0.7_{\rm syst})^\circ$. From the first measurements of the dynamics of $D^+_s\to \eta^{(\prime)}e^+\nu_e$ decays, the products of the hadronic form factors $f_+^{\eta^{(\prime)}}(0)$ and the Cabibbo-Kobayashi-Maskawa matrix element $|V_{cs}|$ are determined with different form factor parameterizations. For the two-parameter series expansion, the results are $f^{\eta}_+(0)|V_{cs}| = 0.4455\pm0.0053_{\rm stat}\pm0.0044_{\rm syst}$ and $f^{\eta^{\prime}}_+(0)|V_{cs}| = 0.477\pm0.049_{\rm stat}\pm0.011_{\rm syst}$., Comment: 10pages, 3 figures
Published: 2019
Full Text: View/download PDF

40. Observation and study of the decay $J/\psi\rightarrow\phi\eta\eta'$

Author: Ablikim, M., Achasov, M. N., Ahmed, S., Albrecht, M., Alekseev, M., Amoroso, A., An, F. F., An, Q., Bai, J. Z., Bai, Y., Bakina, O., Ferroli, R. Baldini, Ban, Y., Begzsuren, K., Bennett, D. W., Bennett, J. V., Berger, N., Bertani, M., Bettoni, D., Bianchi, F., Boger, E., Boyko, I., Briere, R. A., Cai, H., Cai, X., Cakir, O., Calcaterra, A., Cao, G. F., Cetin, S. A., Chai, J., Chang, J. F., Chelkov, G., Chen, G., Chen, H. S., Chen, J. C., Chen, M. L., Chen, P. L., Chen, S. J., Chen, X. R., Chen, Y. B., Cheng, W., Chu, X. K., Cibinetto, G., Cossio, F., Dai, H. L., Dai, J. P., Dbeyssi, A., Dedovich, D., Deng, Z. Y., Denig, A., Denysenko, I., Destefanis, M., De Mori, F., Ding, Y., Dong, C., Dong, J., Dong, L. Y., Dong, M. Y., Dou, Z. L., Du, S. X., Duan, P. F., Fang, J., Fang, S. S., Fang, Y., Farinelli, R., Fava, L., Fegan, S., Feldbauer, F., Felici, G., Feng, C. Q., Fioravanti, E., Fritsch, M., Fu, C. D., Gao, Q., Gao, X. L., Gao, Y., Gao, Y. G., Gao, Z., Garillon, B., Garzia, I., Gilman, A., Goetzen, K., Gong, L., Gong, W. X., Gradl, W., Greco, M., Gu, M. H., Gu, Y. T., Guo, A. Q., Guo, R. P., Guo, Y. P., Guskov, A., Haddadi, Z., Han, S., Hao, X. Q., Harris, F. A., He, K. L., He, X. Q., Heinsius, F. H., Held, T., Heng, Y. K., Hou, Z. L., Hu, H. M., Hu, J. F., Hu, T., Hu, Y., Huang, G. S., Huang, J. S., Huang, X. T., Huang, X. Z., Huang, Z. L., Hussain, T., Andersson, W. Ikegami, Irshad, M., Ji, Q., Ji, Q. P., Ji, X. B., Ji, X. L., Jiang, X. S., Jiang, X. Y., Jiao, J. B., Jiao, Z., Jin, D. P., Jin, S., Jin, Y., Johansson, T., Julin, A., Kalantar-Nayestanaki, N., Kang, X. S., Kavatsyuk, M., Ke, B. C., Keshk, I. K., Khan, T., Khoukaz, A., Kiese, P., Kiuchi, R., Kliemt, R., Koch, L., Kolcu, O. B., Kopf, B., Kornicer, M., Kuemmel, M., Kuessner, M., Kupsc, A., Kurth, M., Kühn, W., Lange, J. S., Larin, P., Lavezzi, L., Leithoff, H., Li, C., Li, Cheng, Li, D. M., Li, F., Li, F. Y., Li, G., Li, H. B., Li, H. J., Li, J. C., Li, J. W., Li, Jin, Li, K. J., Li, Kang, Li, Ke, Li, Lei, Li, P. L., Li, P. R., Li, Q. Y., Li, W. D., Li, W. G., Li, X. L., Li, X. N., Li, X. Q., Li, Z. B., Liang, H., Liang, Y. F., Liang, Y. T., Liao, G. R., Liao, L. Z., Libby, J., Lin, C. X., Lin, D. X., Liu, B., Liu, B. J., Liu, C. X., Liu, D., Liu, D. Y., Liu, F. H., Liu, Fang, Liu, Feng, Liu, H. B., Liu, H. L, Liu, H. M., Liu, Huanhuan, Liu, Huihui, Liu, J. B., Liu, J. Y., Liu, K., Liu, K. Y., Liu, Ke, Liu, L. D., Liu, Q., Liu, S. B., Liu, X., Liu, Y. B., Liu, Z. A., Liu, Zhiqing, Long, Y. F., Lou, X. C., Lu, H. J., Lu, J. G., Lu, Y., Lu, Y. P., Luo, C. L., Luo, M. X., Luo, T., Luo, X. L., Lusso, S., Lyu, X. R., Ma, F. C., Ma, H. L., Ma, L. L., Ma, M. M., Ma, Q. M., Ma, T., Ma, X. N., Ma, X. Y., Ma, Y. M., Maas, F. E., Maggiora, M., Maldaner, S., Malik, Q. A., Mangoni, A., Mao, Y. J., Mao, Z. P., Marcello, S., Meng, Z. X., Messchendorp, J. G., Mezzadri, G., Min, J., Mitchell, R. E., Mo, X. H., Mo, Y. J., Morales, C. Morales, Muchnoi, N. Yu., Muramatsu, H., Mustafa, A., Nefedov, Y., Nerling, F., Nikolaev, I. B., Ning, Z., Nisar, S., Niu, S. L., Niu, X. Y., Olsen, S. L., Ouyang, Q., Pacetti, S., Pan, Y., Papenbrock, M., Patteri, P., Pelizaeus, M., Pellegrino, J., Peng, H. P., Peng, Z. Y., Peters, K., Pettersson, J., Ping, J. L., Ping, R. G., Pitka, A., Poling, R., Prasad, V., Qi, H. R., Qi, M., Qi, T. . Y., Qian, S., Qiao, C. F., Qin, N., Qin, X. S., Qin, Z. H., Qiu, J. F., Qu, S. Q., Rashid, K. H., Redmer, C. F., Richter, M., Ripka, M., Rivetti, A., Rolo, M., Rong, G., Rosner, Ch., Sarantsev, A., Savrié, M., Schoenning, K., Shan, W., Shan, X. Y., Shao, M., Shen, C. P., Shen, P. X., Shen, X. Y., Sheng, H. Y., Shi, X., Song, J. J., Song, W. M., Song, X. Y., Sosio, S., Sowa, C., Spataro, S., Sun, G. X., Sun, J. F., Sun, L., Sun, S. S., Sun, X. H., Sun, Y. J., Sun, Y. K, Sun, Y. Z., Sun, Z. J., Sun, Z. T., Tan, Y. T, Tang, C. J., Tang, G. Y., Tang, X., Tapan, I., Tiemens, M., Tsednee, B., Uman, I., Wang, B., Wang, B. L., Wang, D., Wang, D. Y., Wang, Dan, Wang, K., Wang, L. L., Wang, L. S., Wang, M., Wang, Meng, Wang, P., Wang, P. L., Wang, W. P., Wang, X. F., Wang, X. L., Wang, Y., Wang, Y. F., Wang, Z., Wang, Z. G., Wang, Z. Y., Wang, Zongyuan, Weber, T., Wei, D. H., Weidenkaff, P., Wen, S. P., Wiedner, U., Wolke, M., Wu, L. H., Wu, L. J., Wu, Z., Xia, L., Xia, Y., Xiao, D., Xiao, Y. J., Xiao, Z. J., Xie, Y. G., Xie, Y. H., Xiong, X. A., Xiu, Q. L., Xu, G. F., Xu, J. J., Xu, L., Xu, Q. J., Xu, Q. N., Xu, X. P., Yan, F., Yan, L., Yan, W. B., Yan, W. C., Yan, Y. H., Yang, H. J., Yang, H. X., Yang, L., Yang, R. X., Yang, Y. H., Yang, Y. X., Yang, Yifan, Yang, Z. Q., Ye, M., Ye, M. H., Yin, J. H., You, Z. Y., Yu, B. X., Yu, C. X., Yu, J. S., Yuan, C. Z., Yuan, Y., Yuncu, A., Zafar, A. A., Zeng, Y., Zhang, B. X., Zhang, B. Y., Zhang, C. C., Zhang, D. H., Zhang, H. H., Zhang, H. Y., Zhang, J., Zhang, J. L., Zhang, J. Q., Zhang, J. W., Zhang, J. Y., Zhang, J. Z., Zhang, K., Zhang, L., Zhang, T. J., Zhang, X. Y., Zhang, Y., Zhang, Y. H., Zhang, Y. T., Zhang, Yang, Zhang, Yao, Zhang, Yi, Zhang, Yu, Zhang, Z. H., Zhang, Z. P., Zhang, Z. Y., Zhao, G., Zhao, J. W., Zhao, J. Y., Zhao, J. Z., Zhao, Lei, Zhao, Ling, Zhao, M. G., Zhao, Q., Zhao, S. J., Zhao, T. C., Zhao, Y. B., Zhao, Z. G., Zhemchugov, A., Zheng, B., Zheng, J. P., Zheng, Y. H., Zhong, B., Zhou, L., Zhou, Q., Zhou, X., Zhou, X. K., Zhou, X. R., Zhou, X. Y., Zhou, Xiaoyu, Zhou, Xu, Zhu, A. N., Zhu, J., Zhu, K., Zhu, K. J., Zhu, S., Zhu, S. H., Zhu, X. L., Zhu, Y. C., Zhu, Y. S., Zhu, Z. A., Zhuang, J., Zou, B. S., and Zou, J. H.
Subjects: High Energy Physics - Experiment
Abstract: We report the observation and study of the decay $J/\psi\rightarrow\phi\eta\eta'$ using $1.3\times{10^9}$ $J/\psi$ events collected with the BESIII detector. Its branching fraction, including all possible intermediate states, is measured to be $(2.32\pm0.06\pm0.16)\times{10^{-4}}$. We also report evidence for a structure, denoted as $X$, in the $\phi\eta'$ mass spectrum in the $2.0-2.1$ GeV/$c^2$ region. Using two decay modes of the $\eta'$ meson ($\gamma\pi^+\pi^-$ and $\eta\pi^+\pi^-$), a simultaneous fit to the $\phi\eta'$ mass spectra is performed. Assuming the quantum numbers of the $X$ to be $J^P = 1^-$, its significance is found to be 4.4$\sigma$, with a mass and width of $(2002.1 \pm 27.5 \pm 21.4)$ MeV/$c^2$ and $(129 \pm 17 \pm 9)$ MeV, respectively, and a product branching fraction $\mathcal{B}(J/\psi\rightarrow\eta{}X)\times{}\mathcal{B}(X\rightarrow\phi\eta')=(9.8 \pm 1.2 \pm 1.7)\times10^{-5}$. Alternatively, assuming $J^P = 1^+$, the significance is 3.8$\sigma$, with a mass and width of $(2062.8 \pm 13.1 \pm 7.2)$ MeV/$c^2$ and $(177 \pm 36 \pm 35)$ MeV, respectively, and a product branching fraction $\mathcal{B}(J/\psi\rightarrow\eta{}X)\times{}\mathcal{B}(X\rightarrow\phi\eta')=(9.6 \pm 1.4 \pm 2.0)\times10^{-5}$. The angular distribution of $J/\psi\rightarrow\eta{}X$ is studied and the two $J^P$ assumptions of the $X$ cannot be clearly distinguished due to the limited statistics. In all measurements the first uncertainties are statistical and the second systematic., Comment: 10 pages, 6 figures and 4 tables
Published: 2018
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41. Measurement of the absolute branching fractions of $\Lambda_{c}^{+}\to\Lambda\eta\pi^{+}$ and $\Sigma(1385)^{+}\eta$

Author: Ablikim, M., Achasov, M. N., Ahmed, S., Albrecht, M., Alekseev, M., Amoroso, A., An, F. F., An, Q., Bai, Y., Bakina, O., Ferroli, R. Baldini, Ban, Y., Begzsuren, K., Bennett, D. W., Bennett, J. V., Berger, N., Bertani, M., Bettoni, D., Bianchi, F., Boger, E., Boyko, I., Briere, R. A., Cai, H., Cai, X., Calcaterra, A., Cao, G. F., Cetin, S. A., Chai, J., Chang, J. F., Chang, W. L., Chelkov, G., Chen, G., Chen, H. S., Chen, J. C., Chen, M. L., Chen, S. J., Chen, Y. B., Cheng, W., Cibinetto, G., Cossio, F., Dai, H. L., Dai, J. P., Dbeyssi, A., Dedovich, D., Deng, Z. Y., Denig, A., Denysenko, I., Destefanis, M., De Mori, F., Ding, Y., Dong, C., Dong, J., Dong, L. Y., Dong, M. Y., Dou, Z. L., Du, S. X., Fan, J. Z., Fang, J., Fang, S. S., Fang, Y., Farinelli, R., Fava, L., Feldbauer, F., Felici, G., Feng, C. Q., Fritsch, M., Fu, C. D., Fu, Y., Gao, Q., Gao, X. L., Gao, Y., Gao, Y. G., Gao, Z., Garillon, B., Garzia, I., Gilman, A., Goetzen, K., Gong, L., Gong, W. X., Gradl, W., Greco, M., Gu, L. M., Gu, M. H., Gu, S., Gu, Y. T., Guo, A. Q., Guo, L. B., Guo, R. P., Guo, Y. P., Guskov, A., Haddadi, Z., Han, S., Hao, X. Q., Harris, F. A., He, K. L., Heinsius, F. H., Held, T., Heng, Y. K., Hou, Z. L., Hu, H. M., Hu, J. F., Hu, T., Hu, Y., Huang, G. S., Huang, J. S., Huang, X. T., Huang, X. Z., Huesken, N., Hussain, T., Andersson, W. Ikegami, Imoehl, W., Irshad, M., Ji, Q., Ji, Q. P., Ji, X. B., Ji, X. L., Jiang, H. L., Jiang, X. S., Jiang, X. Y., Jiao, J. B., Jiao, Z., Jin, D. P., Jin, S., Jin, Y., Johansson, T., Kalantar-Nayestanaki, N., Kang, X. S., Kavatsyuk, M., Ke, B. C., Keshk, I. K., Khan, T., Khoukaz, A., Kiese, P., Kiuchi, R., Kliemt, R., Koch, L., Kolcu, O. B., Kopf, B., Kuemmel, M., Kuessner, M., Kupsc, A., Kurth, M., Kühn, W., Lange, J. S., Larin, P., Lavezzi, L., Leithoff, H., Li, C., Li, Cheng, Li, D. M., Li, F., Li, F. Y., Li, G., Li, H. B., Li, H. J., Li, J. C., Li, J. W., Li, Ke, Li, L. K., Li, Lei, Li, P. L., Li, P. R., Li, Q. Y., Li, W. D., Li, W. G., Li, X. L., Li, X. N., Li, X. Q., Li, Z. B., Liang, H., Liang, Y. F., Liang, Y. T., Liao, G. R., Liao, L. Z., Libby, J., Lin, C. X., Lin, D. X., Liu, B., Liu, B. J., Liu, C. X., Liu, D., Liu, D. Y., Liu, F. H., Liu, Fang, Liu, Feng, Liu, H. B., Liu, H. L, Liu, H. M., Liu, Huanhuan, Liu, Huihui, Liu, J. B., Liu, J. Y., Liu, K. Y., Liu, Ke, Liu, Q., Liu, S. B., Liu, X., Liu, Y. B., Liu, Z. A., Liu, Zhiqing, Long, Y. F., Lou, X. C., Lu, H. J., Lu, J. D., Lu, J. G., Lu, Y., Lu, Y. P., Luo, C. L., Luo, M. X., Luo, P. W., Luo, T., Luo, X. L., Lusso, S., Lyu, X. R., Ma, F. C., Ma, H. L., Ma, L. L., Ma, M. M., Ma, Q. M., Ma, X. N., Ma, X. X., Ma, X. Y., Ma, Y. M., Maas, F. E., Maggiora, M., Maldaner, S., Malik, Q. A., Mangoni, A., Mao, Y. J., Mao, Z. P., Marcello, S., Meng, Z. X., Messchendorp, J. G., Mezzadri, G., Min, J., Min, T. J., Mitchell, R. E., Mo, X. H., Mo, Y. J., Morales, C. Morales, Muchnoi, N. Yu., Muramatsu, H., Mustafa, A., Nakhoul, S., Nefedov, Y., Nerling, F., Nikolaev, I. B., Ning, Z., Nisar, S., Niu, S. L., Olsen, S. L., Ouyang, Q., Pacetti, S., Pan, Y., Papenbrock, M., Patteri, P., Pelizaeus, M., Peng, H. P., Peters, K., Pettersson, J., Ping, J. L., Ping, R. G., Pitka, A., Poling, R., Prasad, V., Qi, M., Qi, T. Y., Qian, S., Qiao, C. F., Qin, N., Qin, X. S., Qin, Z. H., Qiu, J. F., Qu, S. Q., Rashid, K. H., Redmer, C. F., Richter, M., Ripka, M., Rivetti, A., Rolo, M., Rong, G., Rosner, Ch., Rump, M., Sarantsev, A., Savrié, M., Schoenning, K., Shan, W., Shan, X. Y., Shao, M., Shen, C. P., Shen, P. X., Shen, X. Y., Sheng, H. Y., Shi, X., Song, J. J., Song, X. Y., Sosio, S., Sowa, C., Spataro, S., Sui, F. F., Sun, G. X., Sun, J. F., Sun, L., Sun, S. S., Sun, X. H., Sun, Y. J., Sun, Y. K, Sun, Y. Z., Sun, Z. J., Sun, Z. T., Tan, Y. T, Tang, C. J., Tang, G. Y., Tang, X., Tiemens, M., Tsednee, B., Uman, I., Wang, B., Wang, B. L., Wang, C. W., Wang, D. Y., Wang, H. H., Wang, K., Wang, L. L., Wang, L. S., Wang, M., Wang, Meng, Wang, P., Wang, P. L., Wang, R. M., Wang, W. P., Wang, X. F., Wang, Y., Wang, Y. F., Wang, Z., Wang, Z. G., Wang, Z. Y., Wang, Zongyuan, Weber, T., Wei, D. H., Weidenkaff, P., Wen, S. P., Wiedner, U., Wolke, M., Wu, L. H., Wu, L. J., Wu, Z., Xia, L., Xia, Y., Xiao, Y. J., Xiao, Z. J., Xie, X. H., Xie, Y. G., Xie, Y. H., Xiong, X. A., Xiu, Q. L., Xu, G. F., Xu, J. J., Xu, L., Xu, Q. J., Xu, W., Xu, X. P., Yan, F., Yan, L., Yan, W. B., Yan, W. C., Yan, Y. H., Yang, H. J., Yang, H. X., Yang, L., Yang, R. X., Yang, S. L., Yang, Y. H., Yang, Y. X., Yang, Yifan, Yang, Z. Q., Ye, M., Ye, M. H., Yin, J. H., You, Z. Y., Yu, B. X., Yu, C. X., Yu, J. S., Yuan, C. Z., Yuan, Y., Yuncu, A., Zafar, A. A., Zeng, Y., Zhang, B. X., Zhang, B. Y., Zhang, C. C., Zhang, D. H., Zhang, H. H., Zhang, H. Y., Zhang, J., Zhang, J. L., Zhang, J. Q., Zhang, J. W., Zhang, J. Y., Zhang, J. Z., Zhang, K., Zhang, L., Zhang, S. F., Zhang, T. J., Zhang, X. Y., Zhang, Y., Zhang, Y. H., Zhang, Y. T., Zhang, Yang, Zhang, Yao, Zhang, Yu, Zhang, Z. H., Zhang, Z. P., Zhang, Z. Y., Zhao, G., Zhao, J. W., Zhao, J. Y., Zhao, J. Z., Zhao, Lei, Zhao, Ling, Zhao, M. G., Zhao, Q., Zhao, S. J., Zhao, T. C., Zhao, Y. B., Zhao, Z. G., Zhemchugov, A., Zheng, B., Zheng, J. P., Zheng, Y. H., Zhong, B., Zhou, L., Zhou, Q., Zhou, X., Zhou, X. K., Zhou, X. R., Zhou, Xiaoyu, Zhou, Xu, Zhu, A. N., Zhu, J., Zhu, K., Zhu, K. J., Zhu, S. H., Zhu, X. L., Zhu, Y. C., Zhu, Y. S., Zhu, Z. A., Zhuang, J., Zou, B. S., and Zou, J. H.
Subjects: High Energy Physics - Experiment
Abstract: We study the decays $\Lambda_{c}^{+}\to\Lambda\eta\pi^{+}$ and $\Sigma(1385)^{+}\eta$ based on $\Lambda_{c}^{+}\bar{\Lambda}_{c}^{-}$ pairs produced in $e^+e^-$ collisions at a center-of-mass energy of $\sqrt{s}=4.6~\mbox{GeV}$, corresponding to an integrated luminosity of $567\;\mbox{pb$^{-1}$}$. The data sample was accumulated with the BESIII detector at the BEPCII collider. The branching fractions are measured to be $\mathcal{B}(\Lambda_{c}^{+} \to \Lambda\eta\pi^{+})=(1.84\pm0.21({\rm{stat.}})\pm0.15({\rm{syst.}}))\%$ and $\mathcal{B}(\Lambda_{c}^{+} \to \Sigma(1385)^{+}\eta)=(0.91\pm0.18({\rm{stat.}})\pm0.09({\rm{syst.}}))\%$, constituting the most precise measurements to date.
Published: 2018
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42. Observation of $e^+e^- \rightarrow D_s^+ \overline{D}{}^{(*)0} K^-$ and study of the $P$-wave $D_s$ mesons

Author: BESIII Collaboration, Ablikim, M., Achasov, M. N., Ahmed, S., Albrecht, M., Alekseev, M., Amoroso, A., An, F. F., An, Q., Bai, J. Z., Bai, Y., Bakina, O., Ferroli, R. Baldini, Ban, Y., Begzsuren, K., Bennett, D. W., Bennett, J. V., Berger, N., Bertani, M., Bettoni, D., Bian, J. M., Bianchi, F., Boger, E., Boyko, I., Briere, R. A., Cai, H., Cai, X., Cakir, O., Calcaterra, A., Cao, G. F., Cetin, S. A., Chai, J., Chang, J. F., Chelkov, G., Chen, G., Chen, H. S., Chen, J. C., Chen, M. L., Chen, P. L., Chen, S. J., Chen, X. R., Chen, Y. B., Chu, X. K., Cibinetto, G., Cossio, F., Dai, H. L., Dai, J. P., Dbeyssi, A., Dedovich, D., Deng, Z. Y., Denig, A., Denysenko, I., Destefanis, M., De Mori, F., Ding, Y., Dong, C., Dong, J., Dong, L. Y., Dong, M. Y., Dou, Z. L., Du, S. X., Duan, P. F., Fang, J., Fang, S. S., Fang, Y., Farinelli, R., Fava, L., Fegan, S., Feldbauer, F., Felici, G., Feng, C. Q., Fioravanti, E., Fritsch, M., Fu, C. D., Gao, Q., Gao, X. L., Gao, Y., Gao, Y. G., Gao, Z., Garillon, B., Garzia, I., Gilman, A., Goetzen, K., Gong, L., Gong, W. X., Gradl, W., Greco, M., Gu, M. H., Gu, Y. T., Guo, A. Q., Guo, R. P., Guo, Y. P., Guskov, A., Haddadi, Z., Han, S., Hao, X. Q., Harris, F. A., He, K. L., He, X. Q., Heinsius, F. H., Held, T., Heng, Y. K., Holtmann, T., Hou, Z. L., Hu, H. M., Hu, J. F., Hu, T., Hu, Y., Huang, G. S., Huang, J. S., Huang, X. T., Huang, X. Z., Huang, Z. L., Hussain, T., Andersson, W. Ikegami, Irshad, M., Ji, Q., Ji, Q. P., Ji, X. B., Ji, X. L., Jiang, X. S., Jiang, X. Y., Jiao, J. B., Jiao, Z., Jin, D. P., Jin, S., Jin, Y., Johansson, T., Julin, A., Kalantar-Nayestanaki, N., Kang, X. S., Kavatsyuk, M., Ke, B. C., Khan, T., Khoukaz, A., Kiese, P., Kliemt, R., Koch, L., Kolcu, O. B., Kopf, B., Kornicer, M., Kuemmel, M., Kuessner, M., Kupsc, A., Kurth, M., Kühn, W., Lange, J. S., Lara, M., Larin, P., Lavezzi, L., Leithoff, H., Li, C., Li, Cheng, Li, D. M., Li, F., Li, F. Y., Li, G., Li, H. B., Li, H. J., Li, J. C., Li, J. W., Li, Jin, Li, K. J., Li, Kang, Li, Ke, Li, Lei, Li, P. L., Li, P. R., Li, Q. Y., Li, W. D., Li, W. G., Li, X. L., Li, X. N., Li, X. Q., Li, Z. B., Liang, H., Liang, Y. F., Liang, Y. T., Liao, G. R., Liao, L. Z., Libby, J., Lin, C. X., Lin, D. X., Liu, B., Liu, B. J., Liu, C. X., Liu, D., Liu, D. Y., Liu, F. H., Liu, Fang, Liu, Feng, Liu, H. B., Liu, H. L, Liu, H. M., Liu, Huanhuan, Liu, Huihui, Liu, J. B., Liu, J. Y., Liu, K., Liu, K. Y., Liu, Kai, Liu, Ke, Liu, L. D., Liu, Q., Liu, S. B., Liu, X., Liu, Y. B., Liu, Z. A., Liu, Zhiqing, Long, Y. F., Lou, X. C., Lu, H. J., Lu, J. G., Lu, Y., Lu, Y. P., Luo, C. L., Luo, M. X., Luo, X. L., Lusso, S., Lyu, X. R., Ma, F. C., Ma, H. L., Ma, L. L., Ma, M. M., Ma, Q. M., Ma, T., Ma, X. N., Ma, X. Y., Ma, Y. M., Maas, F. E., Maggiora, M., Malik, Q. A., Mangoni, A., Mao, Y. J., Mao, Z. P., Marcello, S., Meng, Z. X., Messchendorp, J. G., Mezzadri, G., Min, J., Mitchell, R. E., Mo, X. H., Mo, Y. J., Morales, C. Morales, Muchnoi, N. Yu., Muramatsu, H., Mustafa, A., Nefedov, Y., Nerling, F., Nikolaev, I. B., Ning, Z., Nisar, S., Niu, S. L., Niu, X. Y., Olsen, S. L., Ouyang, Q., Pacetti, S., Pan, Y., Papenbrock, M., Patteri, P., Pelizaeus, M., Pellegrino, J., Peng, H. P., Peng, Z. Y., Peters, K., Pettersson, J., Ping, J. L., Ping, R. G., Pitka, A., Poling, R., Prasad, V., Qi, H. R., Qi, M., Qi, T. . Y., Qian, S., Qiao, C. F., Qin, N., Qin, X. S., Qin, Z. H., Qiu, J. F., Rashid, K. H., Redmer, C. F., Richter, M., Ripka, M., Rolo, M., Rong, G., Rosner, Ch., Sarantsev, A., Savrié, M., Schnier, C., Schoenning, K., Shan, W., Shan, X. Y., Shao, M., Shen, C. P., Shen, P. X., Shen, X. Y., Sheng, H. Y., Shi, X., Song, J. J., Song, W. M., Song, X. Y., Sosio, S., Sowa, C., Spataro, S., Sun, G. X., Sun, J. F., Sun, L., Sun, S. S., Sun, X. H., Sun, Y. J., Sun, Y. K, Sun, Y. Z., Sun, Z. J., Sun, Z. T., Tan, Y. T, Tang, C. J., Tang, G. Y., Tang, X., Tapan, I., Tiemens, M., Toth, D., Tsednee, B., Uman, I., Varner, G. S., Wang, B., Wang, B. L., Wang, D., Wang, D. Y., Wang, Dan, Wang, K., Wang, L. L., Wang, L. S., Wang, M., Wang, Meng, Wang, P., Wang, P. L., Wang, W. P., Wang, X. F., Wang, Y., Wang, Y. F., Wang, Y. Q., Wang, Z., Wang, Z. G., Wang, Z. Y., Wang, Zongyuan, Weber, T., Wei, D. H., Weidenkaff, P., Wen, S. P., Wiedner, U., Wolke, M., Wu, L. H., Wu, L. J., Wu, Z., Xia, L., Xia, Y., Xiao, D., Xiao, Y. J., Xiao, Z. J., Xie, Y. G., Xie, Y. H., Xiong, X. A., Xiu, Q. L., Xu, G. F., Xu, J. J., Xu, L., Xu, Q. J., Xu, Q. N., Xu, X. P., Yan, F., Yan, L., Yan, W. B., Yan, W. C., Yan, Y. H., Yang, H. J., Yang, H. X., Yang, L., Yang, Y. H., Yang, Y. X., Yang, Yifan, Ye, M., Ye, M. H., Yin, J. H., You, Z. Y., Yu, B. X., Yu, C. X., Yu, J. S., Yuan, C. Z., Yuan, Y., Yuncu, A., Zafar, A. A., Zeng, Y., Zeng, Z., Zhang, B. X., Zhang, B. Y., Zhang, C. C., Zhang, D. H., Zhang, H. H., Zhang, H. Y., Zhang, J., Zhang, J. L., Zhang, J. Q., Zhang, J. W., Zhang, J. Y., Zhang, J. Z., Zhang, K., Zhang, L., Zhang, T. J., Zhang, X. Y., Zhang, Y., Zhang, Y. H., Zhang, Y. T., Zhang, Yang, Zhang, Yao, Zhang, Yu, Zhang, Z. H., Zhang, Z. P., Zhang, Z. Y., Zhao, G., Zhao, J. W., Zhao, J. Y., Zhao, J. Z., Zhao, Lei, Zhao, Ling, Zhao, M. G., Zhao, Q., Zhao, S. J., Zhao, T. C., Zhao, Y. B., Zhao, Z. G., Zhemchugov, A., Zheng, B., Zheng, J. P., Zheng, W. J., Zheng, Y. H., Zhong, B., Zhou, L., Zhou, Q., Zhou, X., Zhou, X. K., Zhou, X. R., Zhou, X. Y., Zhu, A. N., Zhu, J., Zhu, K., Zhu, K. J., Zhu, S., Zhu, S. H., Zhu, X. L., Zhu, Y. C., Zhu, Y. S., Zhu, Z. A., Zhuang, J., Zou, B. S., and Zou, J. H.
Subjects: High Energy Physics - Experiment
Abstract: Studies of $e^+e^- \to D_s^+ \overline{D}{}^{(*)0}K^-$ and the $P$-wave charmed-strange mesons are performed based on an $e^+e^-$ collision data sample corresponding to an integrated luminosity of 567 pb$^{-1}$ collected with the BESIII detector at $\sqrt{s}= 4.600$ GeV. The processes of $e^+e^-\to D_s^+ \overline{D}{*}^{0} K^-$ and $D_s^+ \overline{D}{}^{0} K^-$ are observed for the first time and are found to be dominated by the modes $D_s^+ D_{s1}(2536)^-$ and $D_s^+ D^*_{s2}(2573)^-$, respectively. The Born cross sections are measured to be $\sigma^{B}(e^+e^-\to D_s^+ \overline{D}{*}^{0} K^-) = (10.1\pm2.3\pm0.8) pb$ and $\sigma^{B}(e^+e^-\to D_s^+ \overline{D}{}^{0} K^-) = (19.4\pm2.3\pm1.6) pb$, and the products of Born cross section and the decay branching fraction are measured to be $\sigma^{B}(e^+e^-\to D_s^+D_{s1}(2536)^- + c.c.)\cdot\mathcal{B}(D_{s1}(2536)^- \to \overline{D}{*}^{0} K^-) = (7.5 \pm 1.8 \pm 0.7) pb$ and $\sigma^{B}(e^+e^-\to D_s^+ D^*_{s2}(2573)^- + c.c.)\cdot\mathcal{B}(D^*_{s2}(2573)^- \to \overline{D}{}^{0} K^-) = (19.7 \pm 2.9 \pm 2.0) pb$. For the $D_{s1}(2536)^-$ and $D^*_{s2}(2573)^-$ mesons, the masses and widths are measured to be $M(D_{s1}(2536)^-) = (2537.7 \pm 0.5 \pm 3.1)~MeV/c^2,$ $ \Gamma(D_{s1}(2536)^-)) = (1.7\pm 1.2 \pm 0.6)~\rm MeV,$ and $M(D^*_{s2}(2573)^-) = (2570.7\pm 2.0 \pm 1.7)~MeV/c^2,$ $\Gamma(D^*_{s2}(2573)^-) = (17.2 \pm 3.6 \pm 1.1)~\rm MeV.$ The spin-parity of the $D^*_{s2}(2573)^-$ meson is determined to be $J^P=2^{+}$. In addition, the process $e^+e^-\to D_s^+ \overline{D}{}^{(*)0} K^-$ are searched for using the data samples taken at four (two) center-of-mass energies between 4.416 (4.527) and 4.575 GeV, and upper limits at the $90\%$ confidence level on the cross sections are determined.
Published: 2018
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43. Alpha7 nicotinic acetylcholine receptor signaling modulates ovine fetal brain astrocytes transcriptome in response to endotoxin

Author: Cao, M., MacDonald, J. W., Liu, H. L., Weaver, M., Cortes, M., Durosier, L. D., Burns, P., Fecteau, G., Desrochers, A., Schulkin, J., Antonelli, M. C., Bernier, R. A., Dorschner, M., Bammler, T. K., and Frasch, M. G.
Subjects: Quantitative Biology - Genomics, Quantitative Biology - Cell Behavior, Quantitative Biology - Molecular Networks
Abstract: Neuroinflammation in utero may result in lifelong neurological disabilities. Astrocytes play a pivotal role, but the mechanisms are poorly understood. No early postnatal treatment strategies exist to enhance neuroprotective potential of astrocytes. We hypothesized that agonism on alpha7 nicotinic acetylcholine receptor (alpha7nAChR) in fetal astrocytes will augment their neuroprotective transcriptome profile, while the antagonistic stimulation of alpha7nAChR will achieve the opposite. Using an in vivo - in vitro model of developmental programming of neuroinflammation induced by lipopolysaccharide (LPS), we validated this hypothesis in primary fetal sheep astrocytes cultures re-exposed to LPS in presence of a selective alpha7nAChR agonist or antagonist. Our RNAseq findings show that a pro-inflammatory astrocyte transcriptome phenotype acquired in vitro by LPS stimulation is reversed with alpha7nAChR agonistic stimulation. Conversely, antagonistic alpha7nAChR stimulation potentiates the pro-inflammatory astrocytic transcriptome phenotype. Furthermore, we conduct a secondary transcriptome analysis against the identical alpha7nAChR experiments in fetal sheep primary microglia cultures and discuss the implications for neurodevelopment., Comment: See also the accompanying repository on GitHub: https://github.com/martinfrasch/astrocytes_RNAseq
Published: 2018
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44. Observation of $\psi(3686) \to p \bar{p} \eta^{\prime}$ and improved measurement of $J/\psi \to p \bar{p} \eta^{\prime}$

Author: Ablikim, M., Achasov, M. N., Ahmed, S., Albrecht, M., Alekseev, M., Amoroso, A., An, F. F., An, Q., Bai, J. Z., Bai, Y., Bakina, O., Ferroli, R. Baldini, Ban, Y., Begzsuren, K., Bennett, D. W., Bennett, J. V., Berger, N., Bertani, M., Bettoni, D., Bianchi, F., Boger, E., Boyko, I., Briere, R. A., Cai, H., Cai, X., Cakir, O., Calcaterra, A., Cao, G. F., Cetin, S. A., Chai, J., Chang, J. F., Chelkov, G., Chen, G., Chen, H. S., Chen, J. C., Chen, M. L., Chen, P. L., Chen, S. J., Chen, X. R., Chen, Y. B., Cheng, W., Chu, X. K., Cibinetto, G., Cossio, F., Dai, H. L., Dai, J. P., Dbeyssi, A., Dedovich, D., Deng, Z. Y., Denig, A., Denysenko, I., Destefanis, M., De Mori, F., Ding, Y., Dong, C., Dong, J., Dong, L. Y., Dong, M. Y., Dou, Z. L., Du, S. X., Duan, P. F., Fang, J., Fang, S. S., Fang, Y., Farinelli, R., Fava, L., Fegan, S., Feldbauer, F., Felici, G., Feng, C. Q., Fioravanti, E., Fritsch, M., Fu, C. D., Gao, Q., Gao, X. L., Gao, Y., Gao, Y. G., Gao, Z., Garillon, B., Garzia, I., Gilman, A., Goetzen, K., Gong, L., Gong, W. X., Gradl, W., Greco, M., Gu, L. M., Gu, M. H., Gu, Y. T., Guo, A. Q., Guo, L. B., Guo, R. P., Guo, Y. P., Guskov, A., Haddadi, Z., Han, S., Hao, X. Q., Harris, F. A., He, K. L., He, X. Q., Heinsius, F. H., Held, T., Heng, Y. K., Hou, Z. L., Hu, H. M., Hu, J. F., Hu, T., Hu, Y., Huang, G. S., Huang, J. S., Huang, X. T., Huang, X. Z., Huang, Z. L., Hussain, T., Andersson, W. Ikegami, Irshad, M., Ji, Q., Ji, Q. P., Ji, X. B., Ji, X. L., Jiang, X. S., Jiang, X. Y., Jiao, J. B., Jiao, Z., Jin, D. P., Jin, S., Jin, Y., Johansson, T., Julin, A., Kalantar-Nayestanaki, N., Kang, X. S., Kavatsyuk, M., Ke, B. C., Keshk, I. K., Khan, T., Khoukaz, A., Kiese, P., Kiuchi, R., Kliemt, R., Koch, L., Kolcu, O. B., Kopf, B., Kornicer, M., Kuemmel, M., Kuessner, M., Kupsc, A., Kurth, M., Kühn, W., Lange, J. S., Larin, P., Lavezzi, L., Leiber, S., Leithoff, H., Li, C., Li, Cheng, Li, D. M., Li, F., Li, F. Y., Li, G., Li, H. B., Li, H. J., Li, J. C., Li, J. W., Li, K. J., Li, Kang, Li, Ke, Li, Lei, Li, P. L., Li, P. R., Li, Q. Y., Li, T., Li, W. D., Li, W. G., Li, X. L., Li, X. N., Li, X. Q., Li, Z. B., Liang, H., Liang, Y. F., Liang, Y. T., Liao, G. R., Liao, L. Z., Libby, J., Lin, C. X., Lin, D. X., Liu, B., Liu, B. J., Liu, C. X., Liu, D., Liu, D. Y., Liu, F. H., Liu, Fang, Liu, Feng, Liu, H. B., Liu, H. L, Liu, H. M., Liu, Huanhuan, Liu, Huihui, Liu, J. B., Liu, J. Y., Liu, K., Liu, K. Y., Liu, Ke, Liu, L. D., Liu, Q., Liu, S. B., Liu, X., Liu, Y. B., Liu, Z. A., Liu, Zhiqing, Long, Y. F., Lou, X. C., Lu, H. J., Lu, J. G., Lu, Y., Lu, Y. P., Luo, C. L., Luo, M. X., Luo, T., Luo, X. L., Lusso, S., Lyu, X. R., Ma, F. C., Ma, H. L., Ma, L. L., Ma, M. M., Ma, Q. M., Ma, T., Ma, X. N., Ma, X. Y., Ma, Y. M., Maas, F. E., Maggiora, M., Maldaner, S., Malik, Q. A., Mangoni, A., Mao, Y. J., Mao, Z. P., Marcello, S., Meng, Z. X., Messchendorp, J. G., Mezzadri, G., Min, J., Min, T. J., Mitchell, R. E., Mo, X. H., Mo, Y. J., Morales, C. Morales, Muchnoi, N. Yu., Muramatsu, H., Mustafa, A., Nefedov, Y., Nerling, F., Nikolaev, I. B., Ning, Z., Nisar, S., Niu, S. L., Niu, X. Y., Olsen, S. L., Ouyang, Q., Pacetti, S., Pan, Y., Papenbrock, M., Patteri, P., Pelizaeus, M., Pellegrino, J., Peng, H. P., Peng, Z. Y., Peters, K., Pettersson, J., Ping, J. L., Ping, R. G., Pitka, A., Poling, R., Prasad, V., Qi, H. R., Qi, M., Qi, T. Y., Qian, S., Qiao, C. F., Qin, N., Qin, X. S., Qin, Z. H., Qiu, J. F., Qu, S. Q., Rashid, K. H., Redmer, C. F., Richter, M., Ripka, M., Rivetti, A., Rolo, M., Rong, G., Rosner, Ch., Sarantsev, A., Savrié, M., Schoenning, K., Shan, W., Shan, X. Y., Shao, M., Shen, C. P., Shen, P. X., Shen, X. Y., Sheng, H. Y., Shi, X., Song, J. J., Song, W. M., Song, X. Y., Sosio, S., Sowa, C., Spataro, S., Sun, G. X., Sun, J. F., Sun, L., Sun, S. S., Sun, X. H., Sun, Y. J., Sun, Y. K, Sun, Y. Z., Sun, Z. J., Sun, Z. T., Tan, Y. T, Tang, C. J., Tang, G. Y., Tang, X., Tapan, I., Tiemens, M., Tsednee, B., Uman, I., Wang, B., Wang, B. L., Wang, C. W., Wang, D., Wang, D. Y., Wang, Dan, Wang, K., Wang, L. L., Wang, L. S., Wang, M., Wang, Meng, Wang, P., Wang, P. L., Wang, W. P., Wang, X. F., Wang, Y., Wang, Y. F., Wang, Z., Wang, Z. G., Wang, Z. Y., Wang, Zongyuan, Weber, T., Wei, D. H., Weidenkaff, P., Wen, S. P., Wiedner, U., Wolke, M., Wu, L. J., Wu, Z., Xia, L., Xia, X., Xia, Y., Xiao, D., Xiao, Y. J., Xiao, Z. J., Xie, Y. G., Xie, Y. H., Xiong, X. A., Xiu, Q. L., Xu, G. F., Xu, J. J., Xu, L., Xu, Q. J., Xu, Q. N., Xu, X. P., Yan, F., Yan, L., Yan, W. B., Yan, W. C., Yan, Y. H., Yang, H. J., Yang, H. X., Yang, L., Yang, R. X., Yang, Y. H., Yang, Y. X., Yang, Yifan, Yang, Z. Q., Ye, M., Ye, M. H., Yin, J. H., You, Z. Y., Yu, B. X., Yu, C. X., Yu, J. S., Yuan, C. Z., Yuan, Y., Yuncu, A., Zafar, A. A., Zeng, Y., Zhang, B. X., Zhang, B. Y., Zhang, C. C., Zhang, D. H., Zhang, H. H., Zhang, H. Y., Zhang, J., Zhang, J. L., Zhang, J. Q., Zhang, J. W., Zhang, J. Y., Zhang, J. Z., Zhang, K., Zhang, L., Zhang, S. F., Zhang, T. J., Zhang, X. Y., Zhang, Y., Zhang, Y. H., Zhang, Y. T., Zhang, Yang, Zhang, Yao, Zhang, Yu, Zhang, Z. H., Zhang, Z. P., Zhang, Z. Y., Zhao, G., Zhao, J. W., Zhao, J. Y., Zhao, J. Z., Zhao, Lei, Zhao, Ling, Zhao, M. G., Zhao, Q., Zhao, S. J., Zhao, T. C., Zhao, Y. B., Zhao, Z. G., Zhemchugov, A., Zheng, B., Zheng, J. P., Zheng, W. J., Zheng, Y. H., Zhong, B., Zhou, L., Zhou, Q., Zhou, X., Zhou, X. K., Zhou, X. R., Zhou, X. Y., Zhou, Xiaoyu, Zhou, Xu, Zhu, A. N., Zhu, J., Zhu, K., Zhu, K. J., Zhu, S., Zhu, S. H., Zhu, X. L., Zhu, Y. C., Zhu, Y. S., Zhu, Z. A., Zhuang, J., Zou, B. S., and Zou, J. H.
Subjects: High Energy Physics - Experiment
Abstract: We observe the process $\psi(3686) \to p \bar{p} \eta^{\prime}$ for the first time, with a statistical significance higher than 10$\sigma$, and measure the branching fraction of $J/\psi \to p \bar{p} \eta^{\prime}$ with an improved accuracy compared to earlier studies. The measurements are based on $4.48 \times 10^8$ $\psi(3686)$ and $1.31 \times 10^{9}$ $J/\psi$ events collected by the BESIII detector operating at the BEPCII. The branching fractions are determined to be $B(\psi(3686) \to p \bar{p} \eta^{\prime}) = (1.10\pm0.10\pm0.08)\times10^{-5}$ and $B(J/\psi \to p \bar{p} \eta^{\prime})=(1.26\pm0.02\pm 0.07)\times10^{-4}$, where the first uncertainties are statistical and the second ones systematic. Additionally, the $\eta-\eta^{\prime}$ mixing angle is determined to be $-24^{\circ} \pm 11^{\circ}$ based on $\psi(3686) \to p \bar{p} \eta^{\prime}$, and $-24^{\circ} \pm 9^{\circ}$ based on $J/\psi \to p \bar{p} \eta^{\prime}$, respectively., Comment: 9 pages, 20 figures
Published: 2018
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45. Determination of the pseudoscalar decay constant $f_{D_s^+}$ via $D_s^+\to\mu^+\nu_\mu$

Author: BESIII Collaboration, Ablikim, M., Achasov, M. N., Ahmed, S., Albrecht, M., Alekseev, M., Amoroso, A., An, F. F., An, Q., Bai, Y., Bakina, O., Ferroli, R. Baldini, Ban, Y., Begzsuren, K., Bennett, D. W., Bennett, J. V., Berger, N., Bertani, M., Bettoni, D., Bianchi, F., Boyko, I., Briere, R. A., Cai, H., Cai, X., Cakir, O., Calcaterra, A., Cao, G. F., Cetin, S. A., Chai, J., Chang, J. F., Chang, W. L., Chelkov, G., Chen, G., Chen, H. S., Chen, J. C., Chen, M. L., Chen, P. L., Chen, S. J., Chen, Y. B., Cibinetto, G., Cossio, F., Dai, H. L., Dai, J. P., Dbeyssi, A., Dedovich, D., Deng, Z. Y., Denig, A., Denysenko, I., Destefanis, M., De Mori, F., Ding, Y., Dong, C., Dong, J., Dong, L. Y., Dong, M. Y., Dou, Z. L., Du, S. X., Duan, P. F., Fan, J. Z., Fang, J., Fang, S. S., Fang, Y., Farinelli, R., Fava, L., Fegan, S., Feldbauer, F., Felici, G., Feng, C. Q., Fritsch, M., Fu, C. D., Fu, Y., Gao, Q., Gao, X. L., Gao, Y., Gao, Y. G., Gao, Z., Garillon, B., Garzia, I., Gilman, A., Goetzen, K., Gong, L., Gong, W. X., Gradl, W., Greco, M., Gu, L. M., Gu, M. H., Gu, Y. T., Guo, A. Q., Guo, L. B., Guo, R. P., Guo, Y. P., Guskov, A., Haddadi, Z., Han, S., Hao, X. Q., Harris, F. A., He, K. L., Heinsius, F. H., Held, T., Heng, Y. K., Holtmann, T., Hou, Z. L., Hu, H. M., Hu, J. F., Hu, T., Hu, Y., Huang, G. S., Huang, J. S., Huang, X. T., Huang, X. Z., Huang, Z. L., Hussain, T., Andersson, W. Ikegami, Irshad, M., Ji, Q., Ji, Q. P., Ji, X. B., Ji, X. L., Jiang, X. S., Jiang, X. Y., Jiao, J. B., Jiao, Z., Jin, D. P., Jin, S., Jin, Y., Johansson, T., Julin, A., Kalantar-Nayestanaki, N., Kang, X. S., Kavatsyuk, M., Ke, B. C., Khan, T., Khoukaz, A., Kiese, P., Kliemt, R., Koch, L., Kolcu, O. B., Kopf, B., Kornicer, M., Kuemmel, M., Kuessner, M., Kupsc, A., Kurth, M., Kühn, W., Lange, J. S., Lara, M., Larin, P., Lavezzi, L., Leiber, S., Leithoff, H., Li, C., Li, Cheng, Li, D. M., Li, F., Li, F. Y., Li, G., Li, H. B., Li, H. J., Li, J. C., Li, J. W., Li, Ke, Li, Lei, Li, P. L., Li, P. R., Li, Q. Y., Li, T., Li, W. D., Li, W. G., Li, X. L., Li, X. N., Li, X. Q., Li, Z. B., Liang, H., Liang, Y. F., Liang, Y. T., Liao, G. R., Liao, L. Z., Libby, J., Lin, C. X., Lin, D. X., Liu, B., Liu, B. J., Liu, C. X., Liu, D., Liu, D. Y., Liu, F. H., Liu, Fang, Liu, Feng, Liu, H. B., Liu, H. L, Liu, H. M., Liu, Huanhuan, Liu, Huihui, Liu, J. B., Liu, J. Y., Liu, K., Liu, K. Y., Liu, Ke, Liu, Q., Liu, S. B., Liu, X., Liu, Y. B., Liu, Z. A., Liu, Zhiqing, Long, Y. F., Lou, X. C., Lu, H. J., Lu, J. D., Lu, J. G., Lu, Y., Lu, Y. P., Luo, C. L., Luo, M. X., Luo, X. L., Lusso, S., Lyu, X. R., Ma, F. C., Ma, H. L., Ma, L. L., Ma, M. M., Ma, Q. M., Ma, X. N., Ma, X. X., Ma, X. Y., Ma, Y. M., Maas, F. E., Maggiora, M., Malik, Q. A., Mangoni, A., Mao, Y. J., Mao, Z. P., Marcello, S., Meng, Z. X., Messchendorp, J. G., Mezzadri, G., Min, J., Min, T. J., Mitchell, R. E., Mo, X. H., Mo, Y. J., Morales, C. Morales, Morello, G., Muchnoi, N. Yu., Muramatsu, H., Mustafa, A., Nakhoul, S., Nefedov, Y., Nerling, F., Nikolaev, I. B., Ning, Z., Nisar, S., Niu, S. L., Olsen, S. L., Ouyang, Q., Pacetti, S., Pan, Y., Papenbrock, M., Patteri, P., Pelizaeus, M., Pellegrino, J., Peng, H. P., Peters, K., Pettersson, J., Ping, J. L., Ping, R. G., Pitka, A., Poling, R., Prasad, V., Qi, H. R., Qi, M., Qi, T. Y., Qian, S., Qiao, C. F., Qin, N., Qin, X. S., Qin, Z. H., Qiu, J. F., Rashid, K. H., Redmer, C. F., Richter, M., Ripka, M., Rolo, M., Rong, G., Rosner, Ch., Sarantsev, A., Savrié, M., Schnier, C., Schoenning, K., Shan, W., Shan, X. Y., Shao, M., Shen, C. P., Shen, P. X., Shen, X. Y., Sheng, H. Y., Shi, X., Song, J. J., Song, W. M., Song, X. Y., Sosio, S., Sowa, C., Spataro, S., Sun, G. X., Sun, J. F., Sun, L., Sun, S. S., Sun, X. H., Sun, Y. J., Sun, Y. K, Sun, Y. Z., Sun, Z. J., Sun, Z. T., Tan, Y. T, Tang, C. J., Tang, G. Y., Tang, X., Tapan, I., Tiemens, M., Tsednee, B., Uman, I., Varner, G. S., Wang, B., Wang, B. L., Wang, C. W., Wang, D. Y., Wang, Dan, Wang, K., Wang, L. L., Wang, L. S., Wang, M., Wang, Meng, Wang, P., Wang, P. L., Wang, W. P., Wang, X. F., Wang, Y., Wang, Y. F., Wang, Y. Q., Wang, Z., Wang, Z. G., Wang, Z. Y., Wang, Zongyuan, Weber, T., Wei, D. H., Weidenkaff, P., Wen, S. P., Wiedner, U., Wolke, M., Wu, L. H., Wu, L. J., Wu, Z., Xia, L., Xia, X., Xia, Y., Xiao, D., Xiao, Y. J., Xiao, Z. J., Xie, Y. G., Xie, Y. H., Xiong, X. A., Xiu, Q. L., Xu, G. F., Xu, J. J., Xu, L., Xu, Q. J., Xu, Q. N., Xu, X. P., Yan, F., Yan, L., Yan, W. B., Yan, W. C., Yan, Y. H., Yang, H. J., Yang, H. X., Yang, L., Yang, S. L., Yang, Y. H., Yang, Y. X., Yang, Yifan, Ye, M., Ye, M. H., Yin, J. H., You, Z. Y., Yu, B. X., Yu, C. X., Yuan, C. Z., Yuan, Y., Yuncu, A., Zafar, A. A., Zallo, A., Zeng, Y., Zeng, Z., Zhang, B. X., Zhang, B. Y., Zhang, C. C., Zhang, D. H., Zhang, H. H., Zhang, H. Y., Zhang, J., Zhang, J. L., Zhang, J. Q., Zhang, J. W., Zhang, J. Y., Zhang, J. Z., Zhang, K., Zhang, L., Zhang, S. F., Zhang, T. J., Zhang, X. Y., Zhang, Y., Zhang, Y. H., Zhang, Y. T., Zhang, Yang, Zhang, Yao, Zhang, Yu, Zhang, Z. H., Zhang, Z. P., Zhang, Z. Y., Zhao, G., Zhao, J. W., Zhao, J. Y., Zhao, J. Z., Zhao, Lei, Zhao, Ling, Zhao, M. G., Zhao, Q., Zhao, S. J., Zhao, T. C., Zhao, Y. B., Zhao, Z. G., Zhemchugov, A., Zheng, B., Zheng, J. P., Zheng, W. J., Zheng, Y. H., Zhong, B., Zhou, L., Zhou, Q., Zhou, X., Zhou, X. K., Zhou, X. R., Zhou, X. Y., Zhu, A. N., Zhu, J., Zhu, K., Zhu, K. J., Zhu, S., Zhu, S. H., Zhu, X. L., Zhu, Y. C., Zhu, Y. S., Zhu, Z. A., Zhuang, J., Zou, B. S., and Zou, J. H.
Subjects: High Energy Physics - Experiment
Abstract: Using a $3.19~\mathrm{fb}^{-1}$ data sample collected at an $e^+e^-$ center-of-mass energy of $E_{\rm cm}=4.178$ GeV with the BESIII detector, we measure the branching fraction of the leptonic decay $D_s^+\to\mu^+\nu_\mu$ to be $\mathcal{B}_{D_s^+\to\mu^+\nu_\mu}=(5.49\pm0.16_{\rm stat.}\pm0.15_{\rm syst.})\times10^{-3}$. Combining our branching fraction with the masses of the $D_s^+$ and $\mu^+$ and the lifetime of the $D_s^+$, we determine $f_{D_s^+}|V_{cs}|=246.2\pm3.6_{\rm stat.}\pm3.5_{\rm syst.}~\mathrm{MeV}$. Using the $c\to s$ quark mixing matrix element $|V_{cs}|$ determined from a global standard model fit, we evaluate the $D_s^+$ decay constant $f_{D_s^+}=252.9\pm3.7_{\rm stat.}\pm3.6_{\rm syst.}$\,MeV. Alternatively, using the value of $f_{D_s^+}$ calculated by lattice quantum chromodynamics, we find $|V_{cs}| = 0.985\pm0.014_{\rm stat.}\pm0.014_{\rm syst.}$. These values of $\mathcal{B}_{D_s^+\to\mu^+\nu_\mu}$, $f_{D_s^+}|V_{cs}|$, $f_{D_s^+}$ and $|V_{cs}|$ are each the most precise results to date.
Published: 2018
Full Text: View/download PDF

46. Study of the decay $D^0\rightarrow \bar{K}^0\pi^-e^+\nu_e$

Author: Ablikim, M., Achasov, M. N., Ahmed, S., Albrecht, M., Alekseev, M., Amoroso, A., An, F. F., An, Q., Bai, Y., Bakina, O., Ferroli, R. Baldini, Ban, Y., Begzsuren, K., Bennett, D. W., Bennett, J. V., Berger, N., Bertani, M., Bettoni, D., Bianchi, F., Boger, E., Boyko, I., Briere, R. A., Cai, H., Cai, X., Calcaterra, A., Cao, G. F., Cetin, S. A., Chai, J., Chang, J. F., Chang, W. L., Chelkov, G., Chen, G., Chen, H. S., Chen, J. C., Chen, M. L., Chen, P. L., Chen, S. J., Chen, X. R., Chen, Y. B., Cheng, W., Chu, X. K., Cibinetto, G., Cossio, F., Dai, H. L., Dai, J. P., Dbeyssi, A., Dedovich, D., Deng, Z. Y., Denig, A., Denysenko, I., Destefanis, M., De Mori, F., Ding, Y., Dong, C., Dong, J., Dong, L. Y., Dong, M. Y., Dou, Z. L., Du, S. X., Duan, P. F., Fang, J., Fang, S. S., Fang, Y., Farinelli, R., Fava, L., Feldbauer, F., Felici, G., Feng, C. Q., Fritsch, M., Fu, C. D., Gao, Q., Gao, X. L., Gao, Y., Gao, Y. G., Gao, Z., Garillon, B., Garzia, I., Gilman, A., Goetzen, K., Gong, L., Gong, W. X., Gradl, W., Greco, M., Gu, L. M., Gu, M. H., Gu, Y. T., Guo, A. Q., Guo, L. B., Guo, R. P., Guo, Y. P., Guskov, A., Haddadi, Z., Han, S., Hao, X. Q., Harris, F. A., He, K. L., Heinsius, F. H., Held, T., Heng, Y. K., Hou, Z. L., Hu, H. M., Hu, J. F., Hu, T., Hu, Y., Huang, G. S., Huang, J. S., Huang, X. T., Huang, X. Z., Huang, Z. L., Hussain, T., Andersson, W. Ikegami, Imoehl, W., Irshad, M., Ji, Q., Ji, Q. P., Ji, X. B., Ji, X. L., Jiang, H. L., Jiang, X. S., Jiang, X. Y., Jiao, J. B., Jiao, Z., Jin, D. P., Jin, S., Jin, Y., Johansson, T., Kalantar-Nayestanaki, N., Kang, X. S., Kavatsyuk, M., Ke, B. C., Keshk, I. K., Khan, T., Khoukaz, A., Kiese, P., Kiuchi, R., Kliemt, R., Koch, L., Kolcu, O. B., Kopf, B., Kuemmel, M., Kuessner, M., Kupsc, A., Kurth, M., Kühn, W., Lange, J. S., Larin, P., Lavezzi, L., Leiber, S., Leithoff, H., Li, C., Li, Cheng, Li, D. M., Li, F., Li, F. Y., Li, G., Li, H. B., Li, H. J., Li, J. C., Li, J. W., Li, K. J., Li, Kang, Li, Ke, Li, Lei, Li, P. L., Li, P. R., Li, Q. Y., Li, T., Li, W. D., Li, W. G., Li, X. L., Li, X. N., Li, X. Q., Li, Z. B., Liang, H., Liang, Y. F., Liang, Y. T., Liao, G. R., Liao, L. Z., Libby, J., Lin, C. X., Lin, D. X., Liu, B., Liu, B. J., Liu, C. X., Liu, D., Liu, D. Y., Liu, F. H., Liu, Fang, Liu, Feng, Liu, H. B., Liu, H. L, Liu, H. M., Liu, Huanhuan, Liu, Huihui, Liu, J. B., Liu, J. Y., Liu, K. Y., Liu, Ke, Liu, L. D., Liu, Q., Liu, S. B., Liu, X., Liu, Y. B., Liu, Z. A., Liu, Zhiqing, Long, Y. F., Lou, X. C., Lu, H. J., Lu, J. G., Lu, Y., Lu, Y. P., Luo, C. L., Luo, M. X., Luo, P. W., Luo, T., Luo, X. L., Lusso, S., Lyu, X. R., Ma, F. C., Ma, H. L., Ma, L. L., Ma, M. M., Ma, Q. M., Ma, X. N., Ma, X. Y., Ma, Y. M., Maas, F. E., Maggiora, M., Maldaner, S., Malde, S., Malik, Q. A., Mangoni, A., Mao, Y. J., Mao, Z. P., Marcello, S., Meng, Z. X., Messchendorp, J. G., Mezzadri, G., Min, J., Min, T. J., Mitchell, R. E., Mo, X. H., Mo, Y. J., Morales, C. Morales, Muchnoi, N. Yu., Muramatsu, H., Mustafa, A., Nakhoul, S., Nefedov, Y., Nerling, F., Nikolaev, I. B., Ning, Z., Nisar, S., Niu, S. L., Niu, X. Y., Olsen, S. L., Ouyang, Q., Pacetti, S., Pan, Y., Papenbrock, M., Patteri, P., Pelizaeus, M., Pellegrino, J., Peng, H. P., Peng, Z. Y., Peters, K., Pettersson, J., Ping, J. L., Ping, R. G., Pitka, A., Poling, R., Prasad, V., Qi, H. R., Qi, M., Qi, T. Y., Qian, S., Qiao, C. F., Qin, N., Qin, X. S., Qin, Z. H., Qiu, J. F., Qu, S. Q., Rashid, K. H., Redmer, C. F., Richter, M., Ripka, M., Rivetti, A., Rolo, M., Rong, G., Rosner, Ch., Sarantsev, A., Savrié, M., Schoenning, K., Shan, W., Shan, X. Y., Shao, M., Shen, C. P., Shen, P. X., Shen, X. Y., Sheng, H. Y., Shi, X., Song, J. J., Song, W. M., Song, X. Y., Sosio, S., Sowa, C., Spataro, S., Sui, F. F., Sun, G. X., Sun, J. F., Sun, L., Sun, S. S., Sun, X. H., Sun, Y. J., Sun, Y. K, Sun, Y. Z., Sun, Z. J., Sun, Z. T., Tan, Y. T, Tang, C. J., Tang, G. Y., Tang, X., Tiemens, M., Tsednee, B., Uman, I., Wang, B., Wang, B. L., Wang, C. W., Wang, D., Wang, D. Y., Wang, H. H., Wang, K., Wang, L. L., Wang, L. S., Wang, M., Wang, Meng, Wang, P., Wang, P. L., Wang, W. P., Wang, X. F., Wang, Y., Wang, Y. F., Wang, Y. Q., Wang, Z., Wang, Z. G., Wang, Z. Y., Wang, Zongyuan, Weber, T., Wei, D. H., Weidenkaff, P., Wen, S. P., Wiedner, U., Wolke, M., Wu, L. H., Wu, L. J., Wu, Z., Xia, L., Xia, X., Xia, Y., Xiao, D., Xiao, Y. J., Xiao, Z. J., Xie, Y. G., Xie, Y. H., Xiong, X. A., Xiu, Q. L., Xu, G. F., Xu, J. J., Xu, L., Xu, Q. J., Xu, X. P., Yan, F., Yan, L., Yan, W. B., Yan, W. C., Yan, Y. H., Yang, H. J., Yang, H. X., Yang, L., Yang, R. X., Yang, S. L., Yang, Y. H., Yang, Y. X., Yang, Yifan, Yang, Z. Q., Ye, M., Ye, M. H., Yin, J. H., You, Z. Y., Yu, B. X., Yu, C. X., Yu, J. S., Yuan, C. Z., Yuan, Y., Yuncu, A., Zafar, A. A., Zeng, Y., Zhang, B. X., Zhang, B. Y., Zhang, C. C., Zhang, D. H., Zhang, H. H., Zhang, H. Y., Zhang, J., Zhang, J. L., Zhang, J. Q., Zhang, J. W., Zhang, J. Y., Zhang, J. Z., Zhang, K., Zhang, L., Zhang, S. F., Zhang, T. J., Zhang, X. Y., Zhang, Y., Zhang, Y. H., Zhang, Y. T., Zhang, Yang, Zhang, Yao, Zhang, Yu, Zhang, Z. H., Zhang, Z. P., Zhang, Z. Y., Zhao, G., Zhao, J. W., Zhao, J. Y., Zhao, J. Z., Zhao, Lei, Zhao, Ling, Zhao, M. G., Zhao, Q., Zhao, S. J., Zhao, T. C., Zhao, Y. B., Zhao, Z. G., Zhemchugov, A., Zheng, B., Zheng, J. P., Zheng, W. J., Zheng, Y. H., Zhong, B., Zhou, L., Zhou, Q., Zhou, X., Zhou, X. K., Zhou, X. R., Zhou, X. Y., Zhou, Xiaoyu, Zhou, Xu, Zhu, A. N., Zhu, J., Zhu, K., Zhu, K. J., Zhu, S., Zhu, S. H., Zhu, X. L., Zhu, Y. C., Zhu, Y. S., Zhu, Z. A., Zhuang, J., Zou, B. S., and Zou, J. H.
Subjects: High Energy Physics - Experiment
Abstract: We report a study of the decay $D^0 \rightarrow \bar{K}^0\pi^-e^+\nu_{e}$ based on a sample of $2.93~\mathrm{fb}^{-1}$ $e^+e^-$ annihilation data collected at the center-of-mass energy of 3.773~GeV with the BESIII detector at the BEPCII collider. The total branching fraction is determined to be $\mathcal{B}(D^0\rightarrow \bar{K}^0\pi^-e^+\nu_{e})=(1.434\pm0.029({\rm stat.})\pm0.032({\rm syst.}))\%$, which is the most precise to date. According to a detailed analysis of the involved dynamics, we find this decay is dominated with the $K^{*}(892)^-$ contribution and present an improved measurement of its branching fraction to be $\mathcal{B}(D^0\rightarrow K^{*}(892)^-e^+\nu_e)=(2.033\pm0.046({\rm stat.})\pm0.047({\rm syst.}))\%$. We further access their hadronic form-factor ratios for the first time as $r_{V}=V(0)/A_1(0)=1.46\pm0.07({\rm stat.})\pm0.02({\rm syst.})$ and $r_{2}=A_2(0)/A_1(0)=0.67\pm0.06({\rm stat.})\pm0.01({\rm syst.})$. In addition, we observe a significant $\bar{K}^0\pi^-$ $S$-wave component accounting for $(5.51\pm0.97({\rm stat.})\pm0.62({\rm syst.}))\%$ of the total decay rate., Comment: 8 pages, 2 figures
Published: 2018
Full Text: View/download PDF

47. Measurement of $e^{+} e^{-} \rightarrow K^{+} K^{-}$ cross section at $\sqrt{s} = 2.00 - 3.08$ GeV

Author: BESIII Collaboration, Ablikim, M., Achasov, M. N., Ahmed, S., Albrecht, M., Alekseev, M., Amoroso, A., An, F. F., An, Q., Bai, J. Z., Bai, Y., Bakina, O., Ferroli, R. Baldini, Ban, Y., Begzsuren, K., Bennett, D. W., Bennett, J. V., Berger, N., Bertani, M., Bettoni, D., Bianchi, F., Boger, E., Boyko, I., Briere, R. A., Cai, H., Cai, X., Cakir, O., Calcaterra, A., Cao, G. F., Cetin, S. A., Chai, J., Chang, J. F., Chelkov, G., Chen, G., Chen, H. S., Chen, J. C., Chen, M. L., Chen, P. L., Chen, S. J., Chen, X. R., Chen, Y. B., Cheng, W., Chu, X. K., Cibinetto, G., Cossio, F., Dai, H. L., Dai, J. P., Dbeyssi, A., Dedovich, D., Deng, Z. Y., Denig, A., Denysenko, I., Destefanis, M., De Mori, F., Ding, Y., Dong, C., Dong, J., Dong, L. Y., Dong, M. Y., Dou, Z. L., Du, S. X., Duan, P. F., Fang, J., Fang, S. S., Fang, Y., Farinelli, R., Fava, L., Fegan, S., Feldbauer, F., Felici, G., Feng, C. Q., Fioravanti, E., Fritsch, M., Fu, C. D., Gao, Q., Gao, X. L., Gao, Y., Gao, Y. G., Gao, Z., Garillon, B., Garzia, I., Gilman, A., Goetzen, K., Gong, L., Gong, W. X., Gradl, W., Greco, M., Gu, M. H., Gu, Y. T., Guo, A. Q., Guo, R. P., Guo, Y. P., Guskov, A., Haddadi, Z., Han, S., Hao, X. Q., Harris, F. A., He, K. L., He, X. Q., Heinsius, F. H., Held, T., Heng, Y. K., Hou, Z. L., Hu, H. M., Hu, J. F., Hu, T., Hu, Y., Huang, G. S., Huang, J. S., Huang, X. T., Huang, X. Z., Huang, Z. L., Hussain, T., Andersson, W. Ikegami, Irshad, M., Ji, Q., Ji, Q. P., Ji, X. B., Ji, X. L., Jiang, X. S., Jiang, X. Y., Jiao, J. B., Jiao, Z., Jin, D. P., Jin, S., Jin, Y., Johansson, T., Julin, A., Kalantar-Nayestanaki, N., Kang, X. S., Kavatsyuk, M., Ke, B. C., Keshk, I. K., Khan, T., Khoukaz, A., Kiese, P., Kiuchi, R., Kliemt, R., Koch, L., Kolcu, O. B., Kopf, B., Kornicer, M., Kuemmel, M., Kuessner, M., Kupsc, A., Kurth, M., Kühn, W., Lange, J. S., Larin, P., Lavezzi, L., Leithoff, H., Li, C., Li, Cheng, Li, D. M., Li, F., Li, F. Y., Li, G., Li, H. B., Li, H. J., Li, J. C., Li, J. W., Li, Jin, Li, K. J., Li, Kang, Li, Ke, Li, Lei, Li, P. L., Li, P. R., Li, Q. Y., Li, W. D., Li, W. G., Li, X. L., Li, X. N., Li, X. Q., Li, Z. B., Liang, H., Liang, Y. F., Liang, Y. T., Liao, G. R., Liao, L. Z., Libby, J., Lin, C. X., Lin, D. X., Liu, B., Liu, B. J., Liu, C. X., Liu, D., Liu, D. Y., Liu, F. H., Liu, Fang, Liu, Feng, Liu, H. B., Liu, H. L, Liu, H. M., Liu, Huanhuan, Liu, Huihui, Liu, J. B., Liu, J. Y., Liu, K., Liu, K. Y., Liu, Ke, Liu, L. D., Liu, Q., Liu, S. B., Liu, X., Liu, Y. B., Liu, Z. A., Liu, Zhiqing, Long, Y. F., Lou, X. C., Lu, H. J., Lu, J. G., Lu, Y., Lu, Y. P., Luo, C. L., Luo, M. X., Luo, T., Luo, X. L., Lusso, S., Lyu, X. R., Ma, F. C., Ma, H. L., Ma, L. L., Ma, M. M., Ma, Q. M., Ma, T., Ma, X. N., Ma, X. Y., Ma, Y. M., Maas, F. E., Maggiora, M., Maldaner, S., Malik, Q. A., Mangoni, A., Mao, Y. J., Mao, Z. P., Marcello, S., Meng, Z. X., Messchendorp, J. G., Mezzadri, G., Min, J., Mitchell, R. E., Mo, X. H., Mo, Y. J., Morales, C. Morales, Muchnoi, N. Yu., Muramatsu, H., Mustafa, A., Nefedov, Y., Nerling, F., Nikolaev, I. B., Ning, Z., Nisar, S., Niu, S. L., Niu, X. Y., Olsen, S. L., Ouyang, Q., Pacetti, S., Pan, Y., Papenbrock, M., Patteri, P., Pelizaeus, M., Pellegrino, J., Peng, H. P., Peng, Z. Y., Peters, K., Pettersson, J., Ping, J. L., Ping, R. G., Pitka, A., Poling, R., Prasad, V., Qi, H. R., Qi, M., Qi, T. . Y., Qian, S., Qiao, C. F., Qin, N., Qin, X. S., Qin, Z. H., Qiu, J. F., Qu, S. Q., Rashid, K. H., Redmer, C. F., Richter, M., Ripka, M., Rivetti, A., Rolo, M., Rong, G., Rosner, Ch., Sarantsev, A., Savrié, M., Schoenning, K., Shan, W., Shan, X. Y., Shao, M., Shen, C. P., Shen, P. X., Shen, X. Y., Sheng, H. Y., Shi, X., Song, J. J., Song, W. M., Song, X. Y., Sosio, S., Sowa, C., Spataro, S., Sun, G. X., Sun, J. F., Sun, L., Sun, S. S., Sun, X. H., Sun, Y. J., Sun, Y. K, Sun, Y. Z., Sun, Z. J., Tan, Y. T, Tang, C. J., Tang, G. Y., Tang, X., Tapan, I., Tiemens, M., Tsednee, B., Uman, I., Wang, B., Wang, B. L., Wang, D., Wang, D. Y., Wang, Dan, Wang, K., Wang, L. L., Wang, L. S., Wang, M., Wang, Meng, Wang, P., Wang, P. L., Wang, W. P., Wang, X. F., Wang, X. L., Wang, Y., Wang, Y. F., Wang, Z., Wang, Z. G., Wang, Z. Y., Wang, Zongyuan, Weber, T., Wei, D. H., Weidenkaff, P., Wen, S. P., Wiedner, U., Wolke, M., Wu, L. H., Wu, L. J., Wu, Z., Xia, L., Xia, Y., Xiao, D., Xiao, Y. J., Xiao, Z. J., Xie, Y. G., Xie, Y. H., Xiong, X. A., Xiu, Q. L., Xu, G. F., Xu, J. J., Xu, L., Xu, Q. J., Xu, Q. N., Xu, X. P., Yan, F., Yan, L., Yan, W. B., Yan, W. C., Yan, Y. H., Yang, H. J., Yang, H. X., Yang, L., Yang, R. X., Yang, Y. H., Yang, Y. X., Yang, Yifan, Yang, Z. Q., Ye, M., Ye, M. H., Yin, J. H., You, Z. Y., Yu, B. X., Yu, C. X., Yu, J. S., Yuan, C. Z., Yuan, Y., Yuncu, A., Zafar, A. A., Zeng, Y., Zhang, B. X., Zhang, B. Y., Zhang, C. C., Zhang, D. H., Zhang, H. H., Zhang, H. Y., Zhang, J., Zhang, J. L., Zhang, J. Q., Zhang, J. W., Zhang, J. Y., Zhang, J. Z., Zhang, K., Zhang, L., Zhang, T. J., Zhang, X. Y., Zhang, Y., Zhang, Y. H., Zhang, Y. T., Zhang, Yang, Zhang, Yao, Zhang, Yi, Zhang, Yu, Zhang, Z. H., Zhang, Z. P., Zhang, Z. Y., Zhao, G., Zhao, J. W., Zhao, J. Y., Zhao, J. Z., Zhao, Lei, Zhao, Ling, Zhao, M. G., Zhao, Q., Zhao, S. J., Zhao, T. C., Zhao, Y. B., Zhao, Z. G., Zhemchugov, A., Zheng, B., Zheng, J. P., Zheng, Y. H., Zhong, B., Zhou, L., Zhou, Q., Zhou, X., Zhou, X. K., Zhou, X. R., Zhou, X. Y., Zhou, Xiaoyu, Zhou, Xu, Zhu, A. N., Zhu, J., Zhu, K., Zhu, K. J., Zhu, S., Zhu, S. H., Zhu, X. L., Zhu, Y. C., Zhu, Y. S., Zhu, Z. A., Zhuang, J., Zou, B. S., and Zou, J. H.
Subjects: High Energy Physics - Experiment
Abstract: The cross section of the process $e^{+} e^{-} \rightarrow K^{+} K^{-}$ is measured at a number of center-of-mass energies $\sqrt{s}$ from 2.00 to 3.08 GeV with the BESIII detector at the Beijing Electron Positron Collider (BEPCII). The results provide the best precision achieved so far. A resonant structure around 2.2 GeV is observed in the cross section line shape. A Breit-Wigner fit yields a mass of $M=2239.2 \pm 7.1 \pm 11.3$~and a width of $\Gamma=139.8\pm12.3\pm20.6$ MeV, where the first uncertainties are statistical and the second ones are systematic. In addition, the time-like electromagnetic form factor of the kaon is determined at the individual center-of-mass energy points., Comment: 8 figures
Published: 2018
Full Text: View/download PDF

48. Evidence for the decays of $\Lambda^+_{c}\to\Sigma^+\eta$ and $\Sigma^+\eta^\prime$

Author: BESIII Collaboration, Ablikim, M., Achasov, M. N., Ahmed, S., Albrecht, M., Alekseev, M., Amoroso, A., An, F. F., An, Q., Bai, Y., Bakina, O., Ferroli, R. Baldini, Ban, Y., Begzsuren, K., Bennett, D. W., Bennett, J. V., Berger, N., Bertani, M., Bettoni, D., Bianchi, F., Boyko, I., Briere, R. A., Cai, H., Cai, X., Cakir, O., Calcaterra, A., Cao, G. F., Cetin, S. A., Chai, J., Chang, J. F., Chang, W. L., Chelkov, G., Chen, G., Chen, H. S., Chen, J. C., Chen, M. L., Chen, P. L., Chen, S. J., Chen, Y. B., Cheng, W., Cibinetto, G., Cossio, F., Dai, H. L., Dai, J. P., Dbeyssi, A., Dedovich, D., Deng, Z. Y., Denig, A., Denysenko, I., Destefanis, M., De Mori, F., Ding, Y., Dong, C., Dong, J., Dong, L. Y., Dong, M. Y., Dou, Z. L., Du, S. X., Duan, P. F., Fan, J. Z., Fang, J., Fang, S. S., Fang, Y., Farinelli, R., Fava, L., Fegan, S., Feldbauer, F., Felici, G., Feng, C. Q., Fritsch, M., Fu, C. D., Fu, Y., Gao, Q., Gao, X. L., Gao, Y., Gao, Y. G., Gao, Z., Garillon, B., Garzia, I., Gilman, A., Goetzen, K., Gong, L., Gong, W. X., Gradl, W., Greco, M., Gu, L. M., Gu, M. H., Gu, Y. T., Guo, A. Q., Guo, L. B., Guo, R. P., Guo, Y. P., Guskov, A., Haddadi, Z., Han, S., Hao, X. Q., Harris, F. A., He, K. L., Heinsius, F. H., Held, T., Heng, Y. K., Hou, Z. L., Hu, H. M., Hu, J. F., Hu, T., Hu, Y., Huang, G. S., Huang, J. S., Huang, X. T., Huang, X. Z., Huang, Z. L., Hussain, T., Hüsken, N., Andersson, W. Ikegami, Irshad, M., Ji, Q., Ji, Q. P., Ji, X. B., Ji, X. L., Jiang, X. S., Jiang, X. Y., Jiao, J. B., Jiao, Z., Jin, D. P., Jin, S., Jin, Y., Johansson, T., Julin, A., Kalantar-Nayestanaki, N., Kang, X. S., Kavatsyuk, M., Ke, B. C., Keshk, I. K., Khan, T., Khoukaz, A., Kiese, P., Kiuchi, R., Kliemt, R., Koch, L., Kolcu, O. B., Kopf, B., Kornicer, M., Kuemmel, M., Kuessner, M., Kupsc, A., Kurth, M., Kühn, W., Lange, J. S., Larin, P., Lavezzi, L., Leiber, S., Leithoff, H., Li, C., Li, Cheng, Li, D. M., Li, F., Li, F. Y., Li, G., Li, H. B., Li, H. J., Li, J. C., Li, J. W., Li, Ke, Li, Lei, Li, P. L., Li, P. R., Li, Q. Y., Li, T., Li, W. D., Li, W. G., Li, X. L., Li, X. N., Li, X. Q., Li, Z. B., Liang, H., Liang, Y. F., Liang, Y. T., Liao, G. R., Liao, L. Z., Libby, J., Lin, C. X., Lin, D. X., Liu, B., Liu, B. J., Liu, C. X., Liu, D., Liu, D. Y., Liu, F. H., Liu, Fang, Liu, Feng, Liu, H. B., Liu, H. L, Liu, H. M., Liu, Huanhuan, Liu, Huihui, Liu, J. B., Liu, J. Y., Liu, K., Liu, K. Y., Liu, Ke, Liu, Q., Liu, S. B., Liu, X., Liu, Y. B., Liu, Z. A., Liu, Zhiqing, Long, Y. F., Lou, X. C., Lu, H. J., Lu, J. D., Lu, J. G., Lu, Y., Lu, Y. P., Luo, C. L., Luo, M. X., Luo, T., Luo, X. L., Lusso, S., Lyu, X. R., Ma, F. C., Ma, H. L., Ma, L. L., Ma, M. M., Ma, Q. M., Ma, X. N., Ma, X. X., Ma, X. Y., Ma, Y. M., Maas, F. E., Maggiora, M., Maldaner, S., Malik, Q. A., Mangoni, A., Mao, Y. J., Mao, Z. P., Marcello, S., Meng, Z. X., Messchendorp, J. G., Mezzadri, G., Min, J., Min, T. J., Mitchell, R. E., Mo, X. H., Mo, Y. J., Morales, C. Morales, Muchnoi, N. Yu., Muramatsu, H., Mustafa, A., Nakhoul, S., Nefedov, Y., Nerling, F., Nikolaev, I. B., Ning, Z., Nisar, S., Niu, S. L., Olsen, S. L., Ouyang, Q., Pacetti, S., Pan, Y., Papenbrock, M., Patteri, P., Pelizaeus, M., Pellegrino, J., Peng, H. P., Peters, K., Pettersson, J., Ping, J. L., Ping, R. G., Pitka, A., Poling, R., Prasad, V., Qi, H. R., Qi, M., Qi, T. Y., Qian, S., Qiao, C. F., Qin, N., Qin, X. S., Qin, Z. H., Qiu, J. F., Qu, S. Q., Rashid, K. H., Redmer, C. F., Richter, M., Ripka, M., Rivetti, A., Rolo, M., Rong, G., Rosner, Ch., Rump, M., Sarantsev, A., Savrié, M., Schoenning, K., Shan, W., Shan, X. Y., Shao, M., Shen, C. P., Shen, P. X., Shen, X. Y., Sheng, H. Y., Shi, X., Song, J. J., Song, W. M., Song, X. Y., Sosio, S., Sowa, C., Spataro, S., Sun, G. X., Sun, J. F., Sun, L., Sun, S. S., Sun, X. H., Sun, Y. J., Sun, Y. K, Sun, Y. Z., Sun, Z. J., Sun, Z. T., Tan, Y. T, Tang, C. J., Tang, G. Y., Tang, X., Tapan, I., Tiemens, M., Tsednee, B., Uman, I., Wang, B., Wang, B. L., Wang, C. W., Wang, D. Y., Wang, Dan, Wang, K., Wang, L. L., Wang, L. S., Wang, M., Wang, Meng, Wang, P., Wang, P. L., Wang, W. P., Wang, X. F., Wang, Y., Wang, Y. F., Wang, Z., Wang, Z. G., Wang, Z. Y., Wang, Zongyuan, Weber, T., Wei, D. H., Weidenkaff, P., Wen, S. P., Wiedner, U., Wolke, M., Wu, L. H., Wu, L. J., Wu, Z., Xia, L., Xia, X., Xia, Y., Xiao, D., Xiao, Y. J., Xiao, Z. J., Xie, Y. G., Xie, Y. H., Xiong, X. A., Xiu, Q. L., Xu, G. F., Xu, J. J., Xu, L., Xu, Q. J., Xu, Q. N., Xu, X. P., Yan, F., Yan, L., Yan, W. B., Yan, W. C., Yan, Y. H., Yang, H. J., Yang, H. X., Yang, L., Yang, R. X., Yang, S. L., Yang, Y. H., Yang, Y. X., Yang, Yifan, Yang, Z. Q., Ye, M., Ye, M. H., Yin, J. H., You, Z. Y., Yu, B. X., Yu, C. X., Yu, J. S., Yuan, C. Z., Yuan, Y., Yuncu, A., Zafar, A. A., Zeng, Y., Zhang, B. X., Zhang, B. Y., Zhang, C. C., Zhang, D. H., Zhang, H. H., Zhang, H. Y., Zhang, J., Zhang, J. L., Zhang, J. Q., Zhang, J. W., Zhang, J. Y., Zhang, J. Z., Zhang, K., Zhang, L., Zhang, S. F., Zhang, T. J., Zhang, X. Y., Zhang, Y., Zhang, Y. H., Zhang, Y. T., Zhang, Yang, Zhang, Yao, Zhang, Yu, Zhang, Z. H., Zhang, Z. P., Zhang, Z. Y., Zhao, G., Zhao, J. W., Zhao, J. Y., Zhao, J. Z., Zhao, Lei, Zhao, Ling, Zhao, M. G., Zhao, Q., Zhao, S. J., Zhao, T. C., Zhao, Y. B., Zhao, Z. G., Zhemchugov, A., Zheng, B., Zheng, J. P., Zheng, W. J., Zheng, Y. H., Zhong, B., Zhou, L., Zhou, Q., Zhou, X., Zhou, X. K., Zhou, X. R., Zhou, X. Y., Zhou, Xiaoyu, Zhou, Xu, Zhu, A. N., Zhu, J., Zhu, K., Zhu, K. J., Zhu, S., Zhu, S. H., Zhu, X. L., Zhu, Y. C., Zhu, Y. S., Zhu, Z. A., Zhuang, J., Zou, B. S., and Zou, J. H.
Subjects: High Energy Physics - Experiment
Abstract: We study the hadronic decays of $\Lambda_{c}^{+}$ to the final states $\Sigma^{+}\eta$ and $\Sigma^+\eta^\prime$, using an $e^{+}e^{-}$ annihilation data sample of 567 pb$^{-1}$ taken at a center-of-mass energy of 4.6 GeV with the BESIII detector at the BEPCII collider. We find evidence for the decays $\Lambda_{c}^{+}\rightarrow\Sigma^{+}\eta$ and $\Sigma^+\eta^\prime$ with statistical significance of $2.5\sigma$ and $3.2\sigma$, respectively. Normalizing to the reference decays $\Lambda_c^+\to\Sigma^+\pi^0$ and $\Sigma^+\omega$, we obtain the ratios of the branching fractions $\frac{{\mathcal B}(\Lambda_c^+\to\Sigma^+\eta)}{{\mathcal B}(\Lambda_c^+\to\Sigma^+\pi^0)}$ and $\frac{{\mathcal B}(\Lambda_c^+\to\Sigma^+\eta^\prime)}{{\mathcal B}(\Lambda_c^+\to\Sigma^+\omega)}$ to be $0.35 \pm 0.16 \pm 0.03$ and $0.86 \pm 0.34 \pm 0.07$, respectively. The upper limits at the 90\% confidence level are set to be $\frac{{\mathcal B}(\Lambda_c^+\to\Sigma^+\eta)}{{\mathcal B}(\Lambda_c^+\to\Sigma^+\pi^0)}<0.58$ and $\frac{{\mathcal B}(\Lambda_c^+\to\Sigma^+\eta^\prime)}{{\mathcal B}(\Lambda_c^+\to\Sigma^+\omega)}<1.2$. Using BESIII measurements of the branching fractions of the reference decays, we determine $\mathcal B({\Lambda_{c}^{+}\rightarrow\Sigma^{+}\eta})=(0.41\pm0.19\pm0.05)\%$ ($<0.68\%$) and $\mathcal B({\Lambda_{c}^{+}\rightarrow\Sigma^{+}\eta'})=(1.34\pm0.53\pm0.21)\%$ ($<1.9\%$). Here, the first uncertainties are statistical and the second systematic. The obtained branching fraction of $\Lambda_c^+\to\Sigma^+\eta$ is consistent with the previous measurement, and the branching fraction of $\Lambda_{c}^{+}\rightarrow\Sigma^{+}\eta^{\prime}$ is measured for the first time., Comment: Accepted by Chin. Phys. C : Chin. Phys. C 43, 083002, (2019)
Published: 2018
Full Text: View/download PDF

49. First measurement of the form factors in $D^+_{s}\rightarrow K^0 e^+\nu_e$ and $D^+_{s}\rightarrow K^{*0} e^+\nu_e$ decays

Author: BESIII Collaboration, Ablikim, M., Achasov, M. N., Ahmed, S., Albrecht, M., Alekseev, M., Amoroso, A., An, F. F., An, Q., Bai, Y., Bakina, O., Ferroli, R. Baldini, Ban, Y., Begzsuren, K., Bennett, D. W., Bennett, J. V., Berger, N., Bertani, M., Bettoni, D., Bianchi, F., Boger, E., Boyko, I., Briere, R. A., Cai, H., Cai, X., Calcaterra, A., Cao, G. F., Cetin, S. A., Chai, J., Chang, J. F., Chang, W. L., Chelkov, G., Chen, G., Chen, H. S., Chen, J. C., Chen, M. L., Chen, P. L., Chen, S. J., Chen, X. R., Chen, Y. B., Cheng, W., Chu, X. K., Cibinetto, G., Cossio, F., Dai, H. L., Dai, J. P., Dbeyssi, A., Dedovich, D., Deng, Z. Y., Denig, A., Denysenko, I., Destefanis, M., De Mori, F., Ding, Y., Dong, C., Dong, J., Dong, L. Y., Dong, M. Y., Dou, Z. L., Du, S. X., Duan, P. F., Fang, J., Fang, S. S., Fang, Y., Farinelli, R., Fava, L., Fegan, S., Feldbauer, F., Felici, G., Feng, C. Q., Fioravanti, E., Fritsch, M., Fu, C. D., Gao, Q., Gao, X. L., Gao, Y., Gao, Y. G., Gao, Z., Garillon, B., Garzia, I., Gilman, A., Goetzen, K., Gong, L., Gong, W. X., Gradl, W., Greco, M., Gu, L. M., Gu, M. H., Gu, Y. T., Guo, A. Q., Guo, L. B., Guo, R. P., Guo, Y. P., Guskov, A., Haddadi, Z., Han, S., Hao, X. Q., Harris, F. A., He, K. L., He, X. Q., Heinsius, F. H., Held, T., Heng, Y. K., Hou, Z. L., Hu, H. M., Hu, J. F., Hu, T., Hu, Y., Huang, G. S., Huang, J. S., Huang, X. T., Huang, X. Z., Huang, Z. L., Hussain, T., Andersson, W. Ikegami, Irshad, M., Ji, Q., Ji, Q. P., Ji, X. B., Ji, X. L., Jiang, X. S., Jiang, X. Y., Jiao, J. B., Jiao, Z., Jin, D. P., Jin, S., Jin, Y., Johansson, T., Julin, A., Kalantar-Nayestanaki, N., Kang, X. S., Kavatsyuk, M., Ke, B. C., Keshk, I. K., Khan, T., Khoukaz, A., Kiese, P., Kiuchi, R., Kliemt, R., Koch, L., Kolcu, O. B., Kopf, B., Kornicer, M., Kuemmel, M., Kuessner, M., Kupsc, A., Kurth, M., Kühn, W., Lange, J. S., Larin, P., Lavezzi, L., Leiber, S., Leithoff, H., Li, C., Li, Cheng, Li, D. M., Li, F., Li, F. Y., Li, G., Li, H. B., Li, H. J., Li, J. C., Li, J. W., Li, K. J., Li, Kang, Li, Ke, Li, Lei, Li, P. L., Li, P. R., Li, Q. Y., Li, T., Li, W. D., Li, W. G., Li, X. L., Li, X. N., Li, X. Q., Li, Z. B., Liang, H., Liang, Y. F., Liang, Y. T., Liao, G. R., Liao, L. Z., Libby, J., Lin, C. X., Lin, D. X., Liu, B., Liu, B. J., Liu, C. X., Liu, D., Liu, D. Y., Liu, F. H., Liu, Fang, Liu, Feng, Liu, H. B., Liu, H. L, Liu, H. M., Liu, Huanhuan, Liu, Huihui, Liu, J. B., Liu, J. Y., Liu, K. Y., Liu, Ke, Liu, L. D., Liu, Q., Liu, S. B., Liu, X., Liu, Y. B., Liu, Z. A., Liu, Zhiqing, Long, Y. F., Lou, X. C., Lu, H. J., Lu, J. G., Lu, Y., Lu, Y. P., Luo, C. L., Luo, M. X., Luo, T., Luo, X. L., Lusso, S., Lyu, X. R., Ma, F. C., Ma, H. L., Ma, L. L., Ma, M. M., Ma, Q. M., Ma, X. N., Ma, X. Y., Ma, Y. M., Maas, F. E., Maggiora, M., Maldaner, S., Malik, Q. A., Mangoni, A., Mao, Y. J., Mao, Z. P., Marcello, S., Meng, Z. X., Messchendorp, J. G., Mezzadri, G., Min, J., Min, T. J., Mitchell, R. E., Mo, X. H., Mo, Y. J., Morales, C. Morales, Muchnoi, N. Yu., Muramatsu, H., Mustafa, A., Nakhoul, S., Nefedov, Y., Nerling, F., Nikolaev, I. B., Ning, Z., Nisar, S., Niu, S. L., Niu, X. Y., Olsen, S. L., Ouyang, Q., Pacetti, S., Pan, Y., Papenbrock, M., Patteri, P., Pelizaeus, M., Pellegrino, J., Peng, H. P., Peng, Z. Y., Peters, K., Pettersson, J., Ping, J. L., Ping, R. G., Pitka, A., Poling, R., Prasad, V., Qi, H. R., Qi, M., Qi, T. Y., Qian, S., Qiao, C. F., Qin, N., Qin, X. S., Qin, Z. H., Qiu, J. F., Qu, S. Q., Rashid, K. H., Redmer, C. F., Richter, M., Ripka, M., Rivetti, A., Rolo, M., Rong, G., Rosner, Ch., Sarantsev, A., Savrié, M., Schoenning, K., Shan, W., Shan, X. Y., Shao, M., Shen, C. P., Shen, P. X., Shen, X. Y., Sheng, H. Y., Shi, X., Song, J. J., Song, W. M., Song, X. Y., Sosio, S., Sowa, C., Spataro, S., Sun, G. X., Sun, J. F., Sun, L., Sun, S. S., Sun, X. H., Sun, Y. J., Sun, Y. K, Sun, Y. Z., Sun, Z. J., Sun, Z. T., Tan, Y. T, Tang, C. J., Tang, G. Y., Tang, X., Tiemens, M., Tsednee, B., Uman, I., Wang, B., Wang, B. L., Wang, C. W., Wang, D., Wang, D. Y., Wang, Dan, Wang, K., Wang, L. L., Wang, L. S., Wang, M., Wang, Meng, Wang, P., Wang, P. L., Wang, W. P., Wang, X. F., Wang, Y., Wang, Y. F., Wang, Z., Wang, Z. G., Wang, Z. Y., Wang, Zongyuan, Weber, T., Wei, D. H., Weidenkaff, P., Wen, S. P., Wiedner, U., Wolke, M., Wu, L. H., Wu, L. J., Wu, Z., Xia, L., Xia, X., Xia, Y., Xiao, D., Xiao, Y. J., Xiao, Z. J., Xie, Y. G., Xie, Y. H., Xiong, X. A., Xiu, Q. L., Xu, G. F., Xu, J. J., Xu, L., Xu, Q. J., Xu, X. P., Yan, F., Yan, L., Yan, W. B., Yan, W. C., Yan, Y. H., Yang, H. J., Yang, H. X., Yang, L., Yang, R. X., Yang, S. L., Yang, Y. H., Yang, Y. X., Yang, Yifan, Yang, Z. Q., Ye, M., Ye, M. H., Yin, J. H., You, Z. Y., Yu, B. X., Yu, C. X., Yu, J. S., Yuan, C. Z., Yuan, Y., Yuncu, A., Zafar, A. A., Zeng, Y., Zhang, B. X., Zhang, B. Y., Zhang, C. C., Zhang, D. H., Zhang, H. H., Zhang, H. Y., Zhang, J., Zhang, J. L., Zhang, J. Q., Zhang, J. W., Zhang, J. Y., Zhang, J. Z., Zhang, K., Zhang, L., Zhang, S. F., Zhang, T. J., Zhang, X. Y., Zhang, Y., Zhang, Y. H., Zhang, Y. T., Zhang, Yang, Zhang, Yao, Zhang, Yu, Zhang, Z. H., Zhang, Z. P., Zhang, Z. Y., Zhao, G., Zhao, J. W., Zhao, J. Y., Zhao, J. Z., Zhao, Lei, Zhao, Ling, Zhao, M. G., Zhao, Q., Zhao, S. J., Zhao, T. C., Zhao, Y. B., Zhao, Z. G., Zhemchugov, A., Zheng, B., Zheng, J. P., Zheng, W. J., Zheng, Y. H., Zhong, B., Zhou, L., Zhou, Q., Zhou, X., Zhou, X. K., Zhou, X. R., Zhou, X. Y., Zhou, Xiaoyu, Zhou, Xu, Zhu, A. N., Zhu, J., Zhu, K., Zhu, K. J., Zhu, S., Zhu, S. H., Zhu, X. L., Zhu, Y. C., Zhu, Y. S., Zhu, Z. A., Zhuang, J., Zou, B. S., and Zou, J. H.
Subjects: High Energy Physics - Experiment
Abstract: We report on new measurements of Cabibbo-suppressed semileptonic $D_s^+$ decays using $3.19~\mathrm{fb}^{-1}$ of $e^+e^-$ annihilation data sample collected at a center-of-mass energy of 4.178~GeV with the BESIII detector at the BEPCII collider. Our results include branching fractions $\mathcal B({D^+_s\rightarrow K^0 e^+\nu_{e}})=(3.25\pm0.38({\rm stat.})\pm0.16({\rm syst.}))\times10^{-3}$ and $\mathcal B({D^+_s\rightarrow K^{*0} e^+\nu_{e}})=(2.37\pm0.26({\rm stat.})\pm0.20({\rm syst.}))\times10^{-3}$ which are much improved relative to previous measurements, and the first measurements of the hadronic form-factor parameters for these decays. For $D^+_s\rightarrow K^0 e^+\nu_{e}$, we obtain $f_+(0)=0.720\pm0.084({\rm stat.})\pm0.013({\rm syst.})$, and for $D^+_s\rightarrow K^{*0} e^+\nu_{e}$, we find form-factor ratios $r_V=V(0)/A_1(0)=1.67\pm0.34({\rm stat.})\pm0.16({\rm syst.})$ and $r_2=A_2(0)/A_1(0)=0.77\pm0.28({\rm stat.})\pm0.07({\rm syst.})$., Comment: 7 pages, 3 figures
Published: 2018
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50. Observation of $D^+_s\rightarrow p\bar{n}$ and confirmation of its large branching fraction

Author: BESIII Collaboration, Ablikim, M., Achasov, M. N., Ahmed, S., Albrecht, M., Alekseev, M., Amoroso, A., An, F. F., An, Q., Bai, J. Z., Bai, Y., Bakina, O., Ferroli, R. Baldini, Ban, Y., Begzsuren, K., Bennett, D. W., Bennett, J. V., Berger, N., Bertani, M., Bettoni, D., Bianchi, F., Boger, E., Boyko, I., Briere, R. A., Cai, H., Cai, X., Cakir, O., Calcaterra, A., Cao, G. F., Cetin, S. A., Chai, J., Chang, J. F., Chelkov, G., Chen, G., Chen, H. S., Chen, J. C., Chen, M. L., Chen, P. L., Chen, S. J., Chen, X. R., Chen, Y. B., Cheng, W., Chu, X. K., Cibinetto, G., Cossio, F., Dai, H. L., Dai, J. P., Dbeyssi, A., Dedovich, D., Deng, Z. Y., Denig, A., Denysenko, I., Destefanis, M., De Mori, F., Ding, Y., Dong, C., Dong, J., Dong, L. Y., Dong, M. Y., Dou, Z. L., Du, S. X., Duan, P. F., Fang, J., Fang, S. S., Fang, Y., Farinelli, R., Fava, L., Fegan, S., Feldbauer, F., Felici, G., Feng, C. Q., Fioravanti, E., Fritsch, M., Fu, C. D., Gao, Q., Gao, X. L., Gao, Y., Gao, Y. G., Gao, Z., Garillon, B., Garzia, I., Gilman, A., Goetzen, K., Gong, L., Gong, W. X., Gradl, W., Greco, M., Gu, M. H., Gu, Y. T., Guo, A. Q., Guo, R. P., Guo, Y. P., Guskov, A., Haddadi, Z., Han, S., Hao, X. Q., Harris, F. A., He, K. L., He, X. Q., Heinsius, F. H., Held, T., Heng, Y. K., Holtmann, T., Hou, Z. L., Hu, H. M., Hu, J. F., Hu, T., Hu, Y., Huang, G. S., Huang, J. S., Huang, X. T., Huang, X. Z., Huang, Z. L., Hussain, T., Andersson, W. Ikegami, Irshad, M., Ji, Q., Ji, Q. P., Ji, X. B., Ji, X. L., Jiang, X. S., Jiang, X. Y., Jiao, J. B., Jiao, Z., Jin, D. P., Jin, S., Jin, Y., Johansson, T., Julin, A., Kalantar-Nayestanaki, N., Kang, X. S., Kavatsyuk, M., Ke, B. C., Khan, T., Khoukaz, A., Kiese, P., Kiuchi, R., Kliemt, R., Koch, L., Kolcu, O. B., Kopf, B., Kornicer, M., Kuemmel, M., Kuessner, M., Kupsc, A., Kurth, M., Kühn, W., Lange, J. S., Lara, M., Larin, P., Lavezzi, L., Leithoff, H., Li, C., Li, Cheng, Li, D. M., Li, F., Li, F. Y., Li, G., Li, H. B., Li, H. J., Li, J. C., Li, J. W., Li, Jin, Li, K. J., Li, Kang, Li, Ke, Li, Lei, Li, P. L., Li, P. R., Li, Q. Y., Li, W. D., Li, W. G., Li, X. L., Li, X. N., Li, X. Q., Li, Z. B., Liang, H., Liang, Y. F., Liang, Y. T., Liao, G. R., Liao, L. Z., Libby, J., Lin, C. X., Lin, D. X., Liu, B., Liu, B. J., Liu, C. X., Liu, D., Liu, D. Y., Liu, F. H., Liu, Fang, Liu, Feng, Liu, H. B., Liu, H. L, Liu, H. M., Liu, Huanhuan, Liu, Huihui, Liu, J. B., Liu, J. Y., Liu, K., Liu, K. Y., Liu, Ke, Liu, L. D., Liu, Q., Liu, S. B., Liu, X., Liu, Y. B., Liu, Z. A., Liu, Zhiqing, Long, Y. F., Lou, X. C., Lu, H. J., Lu, J. G., Lu, Y., Lu, Y. P., Luo, C. L., Luo, M. X., Luo, X. L., Lusso, S., Lyu, X. R., Ma, F. C., Ma, H. L., Ma, L. L., Ma, M. M., Ma, Q. M., Ma, T., Ma, X. N., Ma, X. Y., Ma, Y. M., Maas, F. E., Maggiora, M., Malik, Q. A., Mangoni, A., Mao, Y. J., Mao, Z. P., Marcello, S., Meng, Z. X., Messchendorp, J. G., Mezzadri, G., Min, J., Mitchell, R. E., Mo, X. H., Mo, Y. J., Morales, C. Morales, Muchnoi, N. Yu., Muramatsu, H., Mustafa, A., Nefedov, Y., Nerling, F., Nikolaev, I. B., Ning, Z., Nisar, S., Niu, S. L., Niu, X. Y., Olsen, S. L., Ouyang, Q., Pacetti, S., Pan, Y., Papenbrock, M., Patteri, P., Pelizaeus, M., Pellegrino, J., Peng, H. P., Peng, Z. Y., Peters, K., Pettersson, J., Ping, J. L., Ping, R. G., Pitka, A., Poling, R., Prasad, V., Qi, H. R., Qi, M., Qi, T. Y., Qian, S., Qiao, C. F., Qin, N., Qin, X. S., Qin, Z. H., Qiu, J. F., Rashid, K. H., Redmer, C. F., Richter, M., Ripka, M., Rivetti, A., Rolo, M., Rong, G., Rosner, Ch., Sarantsev, A., Savrié, M., Schnier, C., Schoenning, K., Shan, W., Shan, X. Y., Shao, M., Shen, C. P., Shen, P. X., Shen, X. Y., Sheng, H. Y., Shi, X., Song, J. J., Song, W. M., Song, X. Y., Sosio, S., Sowa, C., Spataro, S., Sun, G. X., Sun, J. F., Sun, L., Sun, S. S., Sun, X. H., Sun, Y. J., Sun, Y. K, Sun, Y. Z., Sun, Z. J., Sun, Z. T., Tan, Y. T, Tang, C. J., Tang, G. Y., Tang, X., Tapan, I., Tiemens, M., Tsednee, B., Uman, I., Varner, G. S., Wang, B., Wang, B. L., Wang, D., Wang, D. Y., Wang, Dan, Wang, K., Wang, L. L., Wang, L. S., Wang, M., Wang, Meng, Wang, P., Wang, P. L., Wang, W. P., Wang, X. F., Wang, Y., Wang, Y. F., Wang, Y. Q., Wang, Z., Wang, Z. G., Wang, Z. Y., Wang, Zongyuan, Weber, T., Wei, D. H., Weidenkaff, P., Wen, S. P., Wiedner, U., Wolke, M., Wu, L. H., Wu, L. J., Wu, Z., Xia, L., Xia, Y., Xiao, D., Xiao, Y. J., Xiao, Z. J., Xie, Y. G., Xie, Y. H., Xiong, X. A., Xiu, Q. L., Xu, G. F., Xu, J. J., Xu, L., Xu, Q. J., Xu, Q. N., Xu, X. P., Yan, F., Yan, L., Yan, W. B., Yan, W. C., Yan, Y. H., Yang, H. J., Yang, H. X., Yang, L., Yang, Y. H., Yang, Y. X., Yang, Yifan, Yang, Z. Q., Ye, M., Ye, M. H., Yin, J. H., You, Z. Y., Yu, B. X., Yu, C. X., Yu, J. S., Yuan, C. Z., Yuan, Y., Yuncu, A., Zafar, A. A., Zeng, Y., Zeng, Z., Zhang, B. X., Zhang, B. Y., Zhang, C. C., Zhang, D. H., Zhang, H. H., Zhang, H. Y., Zhang, J., Zhang, J. L., Zhang, J. Q., Zhang, J. W., Zhang, J. Y., Zhang, J. Z., Zhang, K., Zhang, L., Zhang, T. J., Zhang, X. Y., Zhang, Y., Zhang, Y. H., Zhang, Y. T., Zhang, Yang, Zhang, Yao, Zhang, Yu, Zhang, Z. H., Zhang, Z. P., Zhang, Z. Y., Zhao, G., Zhao, J. W., Zhao, J. Y., Zhao, J. Z., Zhao, Lei, Zhao, Ling, Zhao, M. G., Zhao, Q., Zhao, S. J., Zhao, T. C., Zhao, Y. B., Zhao, Z. G., Zhemchugov, A., Zheng, B., Zheng, J. P., Zheng, Y. H., Zhong, B., Zhou, L., Zhou, Q., Zhou, X., Zhou, X. K., Zhou, X. R., Zhou, X. Y., Zhou, Xiaoyu, Zhou, Xu, Zhu, A. N., Zhu, J., Zhu, K., Zhu, K. J., Zhu, S., Zhu, S. H., Zhu, X. L., Zhu, Y. C., Zhu, Y. S., Zhu, Z. A., Zhuang, J., Zou, B. S., and Zou, J. H.
Subjects: High Energy Physics - Experiment
Abstract: The baryonic decay $D^+_s\rightarrow p\bar{n}$ is observed, and the corresponding branching fraction is measured to be $(1.21\pm0.10\pm0.05)\times10^{-3}$, where the first uncertainty is statistical and second systematic. The data sample used in this analysis was collected with the BESIII detector operating at the BEPCII $e^+e^-$ double-ring collider with a center-of-mass energy of 4.178~GeV and an integrated luminosity of 3.19~fb$^{-1}$. The result confirms the previous measurement by the CLEO Collaboration and is of greatly improved precision, which may deepen our understanding of the dynamical enhancement of the W-annihilation topology in the charmed meson decays.
Published: 2018
Full Text: View/download PDF

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