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1. Atomic Clock Ensemble in Space

Author: Cacciapuoti, L., Busso, A., Jansen, R., Pataraia, S., Peignier, T., Weinberg, S., Crescence, P., Helm, A., Kehrer, J., Koller, S., Lachaud, R., Niedermaier, T., Esnault, F. -X., Massonnet, D., Goujon, D., Pittet, J., Perri, A., Wang, Q., Liu, S., Schaefer, W., Schwall, T., Prochazka, I., Schlicht, A., Schreiber, U., Laurent, P., Lilley, M., Wolf, P., and Salomon, C.
Subjects: General Relativity and Quantum Cosmology, Astrophysics - Instrumentation and Methods for Astrophysics, Physics - Instrumentation and Detectors
Abstract: The Atomic Clock Ensemble in Space (ACES) mission is developing high performance clocks and links for space to test Einstein's theory of general relativity. From the International Space Station, the ACES payload will distribute a clock signal with fractional frequency stability and accuracy of 1E-16 establishing a worldwide network to compare clocks in space and on the ground. ACES will provide an absolute measurement of Einstein's gravitational redshift, it will search for time variations of fundamental constants, contribute to test topological dark matter models, and perform Standard Model Extension tests. Moreover, the ground clocks connected to the ACES network will be compared over different continents and used to measure geopotential differences at the clock locations. After solving some technical problems, the ACES flight model is now approaching its completion. System tests involving the laser-cooled Cs clock PHARAO, the active H-maser SHM and the on-board frequency comparator FCDP have measured the performance of the clock signal delivered by ACES. The ACES microwave link MWL is currently under test. The single-photon avalanche detector of the optical link ELT has been tested and will now be integrated in the ACES payload. The ACES mission concept, its scientific objectives, and the recent test results are discussed here together with the major milestones that will lead us to the ACES launch., Comment: 12 pages, 8 figures
Published: 2024

2. Nuclear structure of dripline nuclei elucidated through precision mass measurements of $^{23}$Si, $^{26}$P, $^{27,28}$S, and $^{31}$Ar

Author: Yu, Y., Xing, Y. M., Zhang, Y. H., Wang, M., Zhou, X. H., Li, J. G., Li, H. H., Yuan, Q., Niu, Y. F., Huang, Y. N., Geng, J., Guo, J. Y., Chen, J. W., Pei, J. C., Xu, F. R., Litvinov, Yu. A., Blaum, K., de Angelis, G., Tanihata, I., Yamaguchi, T., Zhou, X., Xu, H. S., Chen, Z. Y., Chen, R. J., Deng, H. Y., Fu, C. Y., Ge, W. W., Huang, W. J., Jiao, H. Y., Luo, Y. F., Li, H. F., Liao, T., Shi, J. Y., Si, M., Sun, M. Z., Shuai, P., Tu, X. L., Wang, Q., Xu, X., Yan, X. L., Yuan, Y. J., and Zhang, M.
Subjects: Nuclear Experiment
Abstract: Using the B$\rho$-defined isochronous mass spectrometry technique, we report the first determination of the $^{23}$Si, $^{26}$P, $^{27}$S, and $^{31}$Ar masses and improve the precision of the $^{28}$S mass by a factor of 11. Our measurements confirm that these isotopes are bound and fix the location of the proton dripline in P, S, and Ar. We find that the mirror energy differences of the mirror-nuclei pairs $^{26}$P-$^{26}$Na, $^{27}$P-$^{27}$Mg, $^{27}$S-$^{27}$Na, $^{28}$S-$^{28}$Mg, and $^{31}$Ar-$^{31}$Al deviate significantly from the values predicted assuming mirror symmetry. In addition, we observe similar anomalies in the excited states, but not in the ground states, of the mirror-nuclei pairs $^{22}$Al-$^{22}$F and $^{23}$Al-$^{23}$Ne. Using $ab~ initio$ VS-IMSRG and mean field calculations, we show that such a mirror-symmetry breaking phenomeon can be explained by the extended charge distributions of weakly-bound, proton-rich nuclei. When observed, this phenomenon serves as a unique signature that can be valuable for identifying proton-halo candidates.
Published: 2024

3. eDIG-CHANGES III: the lagging eDIG revealed by multi-slit spectroscopy of NGC 891

Author: Lu, Li-Yuan, Li, Jiang-Tao, Vargas, Carlos J., Fang, Taotao, Benjamin, Robert A., Bregman, Joel N., Dettmar, Ralf-Jürgen, English, Jayanne, Heald, George H., Jiang, Yan, Wang, Q. Daniel, and Yang, Yang
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: The kinematic information of the extraplanar diffuse ionized gas (eDIG) around galaxies provides clues to the origin of the gas. The eDIG-CHANGES project studies the physical and kinematic properties of the eDIG around the CHANG-ES sample of nearby edge-on disk galaxies. We use a novel multi-slit narrow-band spectroscopy technique to obtain the spatial distribution of spectral properties of the ionized gas around NGC 891, which is often regarded as an analog of the Milky Way. We developed specific data reduction procedures for the multi-slit narrow-band spectroscopy data taken with the MDM 2.4m telescope. The data presented in this paper covers the H$\alpha$ and [N II]$\lambda\lambda$6548,6583\AA emission lines. The eDIG traced by the H$\alpha$ and [N II] lines shows an obvious asymmetric morphology, being brighter in the northeastern part of the galactic disk and extending a few kpc above and below the disk. Global variations in the [N II]/H$\alpha$ line ratio suggest additional heating mechanisms for the eDIG at large heights beyond photoionization. We also construct position-velocity (PV) diagrams of the eDIG based on our optical multi-slit spectroscopy data and compare them to similar PV diagrams constructed with the H I data. The dynamics of the two gas phases are generally consistent with each other. Modeling the rotation curves at different heights from the galactic mid-plane suggests a vertical negative gradient in turnover radius and maximum rotation velocity, with magnitudes of approximately $3$ kpc kpc$^{-1}$ and $22-25$ km s$^{-1}$ kpc$^{-1}$, respectively. Measured vertical gradients of the rotation curve parameters suggest significant differential rotation of the ionized gas in the halo, or often referred to as the lagging eDIG. Systematic study of the lagging eDIG in our eDIG-CHANGES project, will help us to better understand the dynamics of the ionized gas in the halo., Comment: 11 pages, 8 figures, accepted for publication in A&A
Published: 2024

4. CHANG-ES XXXIV: a 20 kpc radio bubble in the halo of the star-forming galaxy NGC 4217

Author: Heesen, V., Wiegert, T., Irwin, J., Crocker, R., Kiehn, A., Li, J. -T., Wang, Q. D., Stein, M., Dettmar, R. -J., Soida, M., Henriksen, R., Gajovic, L., Yang, Y., and Brüggen, M.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: Cosmic rays may be dynamically very important in driving large-scale galactic winds. Edge-on galaxies give us an outsider's view of the radio halo, which shows the presence of extra-planar cosmic-ray electrons and magnetic fields. We present a new radio continuum imaging study of the nearby edge-on galaxy NGC 4217 in order to study the distribution of extra-planar cosmic rays and magnetic fields. We both observe with the Jansky Very Large Array (JVLA) in the S-band (2-4 GHz) and with LOw Frequency ARray (LOFAR) at 144 MHz. We measure vertical intensity profiles and exponential scale heights. We re-image both JVLA and LOFAR data at matched angular resolution in order to measure radio spectral indices between 144 MHz and 3 GHz. Confusing point-like sources were subtracted prior to imaging. Intensity profiles are then fitted with cosmic-ray electron advection models, where we use an isothermal wind model that is driven by a combination of pressure from the hot gas and cosmic rays. We discover a large-scale radio halo on one (northwestern) side of the galactic disc. The morphology is reminiscent of a bubble extending up to 20 kpc away from the disc. We find spectral ageing in the bubble which allows us to measure advection speeds of the cosmic-ray electrons accelerating from 300 to 600 $\rm km\, s^{-1}$ . Assuming energy equipartition between the cosmic rays and the magnetic field, we estimate the bubble can be inflated by a modest 10 per cent of the kinetic energy injected by supernovae over its dynamical time-scale of 35 Myr. While no active galactic nucleus (AGN) has been detected, such activity in the recent past cannot be ruled out. Non-thermal bubbles with sizes of tens of kiloparsec may be a ubiquitous feature of star-forming galaxies showing the influence of feedback. To determine possible contributions by AGN feedback, will require deeper observations., Comment: Accepted to Astronomy and Astrophysics. 9 pages, 7 figures, 1 table
Published: 2024

5. Disruption of a massive molecular cloud by a supernova in the Galactic Centre: Initial results from the ACES project

Author: Nonhebel, M., Barnes, A. T., Immer, K., Armijos-Abendaño, J., Bally, J., Battersby, C., Burton, M. G., Butterfield, N., Colzi, L., García, P., Ginsburg, A., Henshaw, J. D., Hu, Y., Jiménez-Serra, I., Klessen, R. S., Kruijssen, J. M. D., Liang, F. -H., Longmore, S. N., Lu, X., Martín, S., Mills, E. A. C., Nogueras-Lara, F., Petkova, M. A., Pineda, J. E., Rivilla, V. M., Sánchez-Monge, Á., Santa-Maria, M. G., Smith, H. A., Sofue, Y., Sormani, M. C., Tolls, V., Walker, D. L., Wallace, J., Wang, Q. D., Williams, G. M., and Xu, F. -W.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: The Milky Way's Central Molecular Zone (CMZ) differs dramatically from our local solar neighbourhood, both in the extreme interstellar medium conditions it exhibits (e.g. high gas, stellar, and feedback density) and in the strong dynamics at play (e.g. due to shear and gas influx along the bar). Consequently, it is likely that there are large-scale physical structures within the CMZ that cannot form elsewhere in the Milky Way. In this paper, we present new results from the Atacama Large Millimeter/submillimeter Array (ALMA) large programme ACES (ALMA CMZ Exploration Survey) and conduct a multi-wavelength and kinematic analysis to determine the origin of the M0.8$-$0.2 ring, a molecular cloud with a distinct ring-like morphology. We estimate the projected inner and outer radii of the M0.8$-$0.2 ring to be 79" and 154", respectively (3.1 pc and 6.1 pc at an assumed Galactic Centre distance of 8.2 kpc) and calculate a mean gas density $> 10^{4}$ cm$^{-3}$, a mass of $\sim$ $10^6$ M$_\odot$, and an expansion speed of $\sim$ 20 km s$^{-1}$, resulting in a high estimated kinetic energy ($> 10^{51}$ erg) and momentum ($> 10^7$ M$_\odot$ km s$^{-1}$). We discuss several possible causes for the existence and expansion of the structure, including stellar feedback and large-scale dynamics. We propose that the most likely cause of the M0.8$-$0.2 ring is a single high-energy hypernova explosion. To viably explain the observed morphology and kinematics, such an explosion would need to have taken place inside a dense, very massive molecular cloud, the remnants of which we now see as the M0.8$-$0.2 ring. In this case, the structure provides an extreme example of how supernovae can affect molecular clouds., Comment: 17 pages, 13 figures, and 2 tables. Published in Astronomy & Astrophysics
Published: 2024

6. Ionization potential of radium monofluoride

Author: Wilkins, S. G., Perrett, H. A., Udrescu, S. M., Kyuberis, A. A., Pašteka, L. F., Au, M., Belošević, I., Berger, R., Binnersley, C. L., Bissell, M. L., Borschevsky, A., Breier, A. A., Brinson, A. J., Chrysalidis, K., Cocolios, T. E., Cooper, B. S., de Groote, R. P., Dorne, A., Eliav, E., Field, R. W., Flanagan, K. T., Franchoo, S., Ruiz, R. F. Garcia, Gaul, K., Geldhof, S., Giesen, T. F., Gustafsson, F. P., Hanstorp, D., Heinke, R., Koszorús, Á., Kujanpää, S., Lalanne, L., Neyens, G., Nichols, M., Reilly, J. R., Ricketts, C. M., Rothe, S., Sunaga, A., Borne, B. van den, Vernon, A. R., Wang, Q., Wessolek, J., Wienholtz, F., Yang, X. F., Zhou, Y., and Zülch, C.
Subjects: Physics - Atomic Physics, Nuclear Experiment, Physics - Chemical Physics, Physics - Computational Physics
Abstract: The ionization potential (IP) of radium monofluoride (RaF) was measured to be 4.969(2)[10] eV, revealing a relativistic enhancement in the series of alkaline earth monofluorides. The results are in agreement with a relativistic coupled-cluster prediction of 4.969[7] eV, incorporating up to quantum electrodynamics corrections. Using the same computational methodology, an improved calculation for the dissociation energy ($D_{0}$) of 5.54[5] eV is presented. This confirms that radium monofluoride joins the small group of diatomic molecules for which $D_{0}>\mathrm{IP}$, paving the way for precision control and interrogation of its Rydberg states.
Published: 2024

7. Massive stars exploding in a He-rich circumstellar medium $-$ X. Flash spectral features in the Type Ibn SN 2019cj and observations of SN 2018jmt

Author: Wang, Z. -Y., Pastorello, A., Maeda, K., Reguitti, A., Cai, Y. -Z., Howell, D. Andrew, Benetti, S., Buckley, D., Cappellaro, E., Carini, R., Cartier, R., Chen, T. -W., Elias-Rosa, N., Fang, Q. -L., Gal-Yam, A., Gangopadhyay, A., Gromadzki, M., Gan, W. -P., Hiramatsu, D., Hu, M. -K., Inserra, C., McCully, C., Nicholl, M., Olivares, F. E., Pignata, G., Pineda-Garc'ia, J., Pursiainen, M., Ragosta, F., Rau, A., Roy, R., Sollerman, J., Tartaglia, L., Terreran, G., Valerin, G., Wang, Q., Wang, S. -Q., Young, D. R., Aryan, A., Bronikowski, M., Concepcion, E., Galbany, L., Lin, H., Melandri, A., Petrushevska, T., Ramirez, M., Shi, D. -D, Warwick, B., Zhang, J. -J., Wang, B., Wang, X. -F., and Zhu, X. -J.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Solar and Stellar Astrophysics
Abstract: We present optical and near-infrared observations of two Type Ibn supernovae (SNe), SN 2018jmt and SN 2019cj. Their light curves have rise times of about 10 days, reaching an absolute peak magnitude of $M_g$(SN 2018jmt) = $-$19.07 $\pm$ 0.37 and $M_V$(SN 2019cj) = $-$18.94 $\pm$ 0.19 mag, respectively. The early-time spectra of SN 2018jmt are dominated by a blue continuum, accompanied by narrow (600$-$1000 km~s$^{-1}$) He I lines with P-Cygni profile. At later epochs, the spectra become more similar to those of the prototypical SN Ibn 2006jc. At early phases, the spectra of SN 2019cj show flash ionisation emission lines of C III, N III and He II superposed on a blue continuum. These features disappear after a few days, and then the spectra of SN 2019cj evolve similarly to those of SN 2018jmt. The spectra indicate that the two SNe exploded within a He-rich circumstellar medium (CSM) lost by the progenitors a short time before the explosion. We model the light curves of the two SNe Ibn to constrain the progenitor and the explosion parameters. The ejecta masses are consistent with either that expected for a canonical SN Ib ($\sim$ 2 M$_{\odot}$) or those from a massive WR star ($>$ $\sim$ 4 M$_{\odot}$), with the kinetic energy on the order of $10^{51}$ erg. The lower limit on the ejecta mass ($>$ $\sim$ 2 M$_{\odot}$) argues against a scenario involving a relatively low-mass progenitor (e.g., $M_{ZAMS}$ $\sim$ 10 M$_{\odot}$). We set a conservative upper limit of $\sim$0.1 M$_{\odot}$ for the $^{56}$Ni masses in both SNe. From the light curve modelling, we determine a two-zone CSM distribution, with an inner, flat CSM component, and an outer CSM with a steeper density profile. The physical properties of SN 2018jmt and SN 2019cj are consistent with those expected from the core collapse of relatively massive, stripped-envelope (SE) stars., Comment: 28 pages, 19 figures, Accepted for publication in Astronomy & Astrophysics
Published: 2024
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8. The RAdio Galaxy Environment Reference Survey (RAGERS): Evidence of an anisotropic distribution of submillimeter galaxies in the 4C 23.56 protocluster at z=2.48

Author: Zhou, Dazhi, Greve, Thomas R., Gullberg, Bitten, Lee, Minju M., Di Mascolo, Luca, Dicker, Simon R., Romero, Charles E., Chapman, Scott C., Chen, Chian-Chou, Cornish, Thomas, Devlin, Mark J., Ho, Luis C., Kohno, Kotaro, Lagos, Claudia D. P., Mason, Brian S., Mroczkowski, Tony, Wagg, Jeff F. W., Wang, Q. Daniel, Wang, Ran, Brinch, Malte., Dannerbauer, Helmut, Jiang, Xue-Jian, Lauritsen, Lynge R. B., Vijayan, Aswin P., Vizgan, David, Wardlow, Julie L., Sarazin, Craig L., Sarmiento, Karen P., Serjeant, Stephen, Bhandarkar, Tanay A., Haridas, Saianeesh K., Moravec, Emily, Orlowski-Scherer, John, Sievers, Jonathan L. R., Tanaka, Ichi, Wang, Yu-Jan, Zeballos, Milagros, Laza-Ramos, Andres, Liu, Yuanqi, Hassan, Mohd Shaiful Rizal, Jwel, Abdul Kadir Md, Nazri, Affan Adly, Lim, Ming-Kang, and Ibrahim, Ungku Ferwani Salwa Ungku
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: High-redshift radio(-loud) galaxies (H$z$RGs) are massive galaxies with powerful radio-loud active galactic nuclei (AGNs) and serve as beacons for protocluster identification. However, the interplay between H$z$RGs and the large-scale environment remains unclear. To understand the connection between H$z$RGs and the surrounding obscured star formation, we investigated the overdensity and spatial distribution of submillimeter-bright galaxies (SMGs) in the field of 4C\,23.56, a well-known H$z$RG at $z=2.48$. We used SCUBA-2 data ($\sigma\,{\sim}\,0.6$\,mJy) to estimate the $850\,{\rm \mu m}$ source number counts and examine the radial and azimuthal overdensities of the $850\,{\rm \mu m}$ sources in the vicinity of the H$z$RG. The angular distribution of SMGs is inhomogeneous around the H$z$RG 4C\,23.56, with fewer sources oriented along the radio jet. We also find a significant overdensity of bright SMGs (${\rm S}_{850\rm\,\mu m}\geq5\,$mJy). Faint and bright SMGs exhibit different spatial distributions. The former are concentrated in the core region, while the latter prefer the outskirts of the H$z$RG field. High-resolution observations show that the seven brightest SMGs in our sample are intrinsically bright, suggesting that the overdensity of bright SMGs is less likely due to the source multiplicity., Comment: 19 pages, 17 figures, 5 tables, accepted to A&A
Published: 2024

9. CHANG-ES XXXII: Spatially Resolved Thermal/Nonthermal Separation from Radio Data Alone -- New Probes into NGC 3044 and NGC 5775

Author: Irwin, Judith, Cook, Tanden, Stein, Michael, Dettmar, Ralf-Juergen, Heesen, Volker, Wang, Q. Daniel, Wiegert, Theresa, Stein, Yelena, and Vargas, Carlos
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We have carried out spatially resolved thermal/nonthermal separation on two edge-on galaxies, NGC~3044 and NGC~5775, using only radio data. Narrow-band imaging within a frequency band that is almost contiguous from 1.25 to 7.02 GHz (L-band, S-band and C-band) has allowed us to fit spectra and construct thermal, nonthermal, and nonthermal spectral index maps. This method does not require any ancillary H$\alpha$ and infrared data, or reliance on dust corrections that are challenging in edge-on galaxies. For NGC~3044, at 15 arcsec resolution, we find a median thermal fraction of $\sim\, 13$\% with an estimated uncertainty in this fraction of $\sim\, 50$\% at 4.13 GHz. This compares well with the H$\alpha$ mixture method results. We uncovered evidence for a vertical outflow feature reaching at least $z\,\sim\,3.5$ kpc in projection above the plane, reminiscent of M82's starburst wind. For the higher SFR galaxy, NGC~5775 at 12 arcsec resolution, we find a median thermal fraction of 44\% at 4.13 GHz with an estimated error on this fraction of 17\%. Both galaxies show a change of slope (flattening) in L-band. These results suggest that a radio-only method for separating thermal from nonthermal emission is not only feasible, but able to reveal new features that might otherwise be obscured in edge-on disks., Comment: Accepted to AJ on July 18, 2024
Published: 2024
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10. Dynamic phase transition into a mixed-CDW state in 1$T$-TaS$_2$ via a thermal quench

Author: de la Torre, A., Wang, Q., Campbell, B., Riffle, J. V., Balasundaram, D., Vora, P. M., Ruff, J. P. C., Hollen, S. M., and Plumb, K. W.
Subjects: Condensed Matter - Materials Science
Abstract: Ultrafast light-matter interaction has emerged as a new mechanism to exert control over the macroscopic properties of quantum materials toward novel functionality. To date, technological applications of these non-thermal phases are limited by their ultrashort lifetimes and low-ordering temperatures. Among the most studied photoinduced metastable phases for their technological promise is the hidden metallic charge density wave (H-CDW) in the model correlated CDW compound 1$T$-TaS$_2$. Despite active study and engineering, the nature of the photoinduced H-CDW remains the subject of debate and is only accessible at cryogenic temperatures. Here, we stabilize the H-CDW phase at thermal equilibrium up to near-room temperature by accessing an intermediate mixed CDW order regime via thermal quenching. Using x-ray high dynamic range reciprocal space mapping (HDRM) and scanning tunneling spectroscopy (STS), we reveal the coexistence of commensurate (C) CDW and H-CDW domains below 180 K during cooling and below 210 K during warming. Our findings show that each order parameter breaks basal plane mirror symmetry with different chiral orientations and induces out-of-plane unit cell tripling in the H-CDW phase. Despite metallic domain walls and a finite density of states at zero bias observed via STS, bulk resistance remains insulating due to CDW stacking disorder. This study establishes the H-CDW as a thermally stable phase and introduces a new mechanism for switchable metallic behavior in thin flakes of 1$T$-TaS$_2$ and similar materials with competing order phases.
Published: 2024

11. Imaging of single barium atoms in a second matrix site in solid xenon for barium tagging in a $^{136}$Xe double beta decay experiment

Author: Yvaine, M., Fairbank, D., Soderstrom, J., Taylor, C., Stanley, J., Walton, T., Chambers, C., Iverson, A., Fairbank, W., Kharusi, S. Al, Amy, A., Angelico, E., Anker, A., Arnquist, I. J., Atencio, A., Bane, J., Belov, V., Bernard, E. P., Bhatta, T., Bolotnikov, A., Breslin, J., Breur, P. A., Brodsky, J. P., Brown, E., Brunner, T., Caden, E., Cao, G. F., Cesmecioglu, D., Chambers, E., Chana, B., Chernyak, D., Chiu, M., Collister, R., Cvitan, M., Daniels, T., Darroch, L., DeVoe, R., di Vacri, M. L., Dolinski, M. J., Eckert, B., Elbeltagi, M., Elmansali, R., Fatemighomi, N., Foust, B., Fu, Y. S., Gallacher, D., Gallice, N., Giacomini, G., Gillis, W., Gingras, C., Gornea, R., Gratta, G., Hardy, C. A., Hedges, S., Hein, E., Holt, J. D., Hoppe, E. W., Karelin, A., Keblbeck, D., Kotov, I., Kuchenkov, A., Kumar, K. S., Kwiatkowski, A. A., Larson, A., Latif, M. B., Leach, K. G., Lennarz, A., Leonard, D. S., Lewis, H., Li, G., Li, Z., Licciardi, C., Lindsay, R., MacLellan, R., Majidi, S., Malbrunot, C., Masbou, J., McMichael, K., Peregrina, M. Medina, Moe, M., Mong, B., Moore, D. C., Natzke, C. R., Ngwadla, X. E., Ni, K., Nolan, A., Nowicki, S. C., Ondze, J. C. Nzobadila, Odian, A., Orrell, J. L., Ortega, G. S., Overman, C. T., Pagani, L., Smalley, H. Peltz, Perna, A., Pocar, A., Radeka, V., Raguzin, E., Rasiwala, H., Ray, D., Rescia, S., Richardson, G., Ross, R., Rowson, P. C., Saldanha, R., Sangiorgio, S., Schwartz, S., Sekula, S., Si, L., Soma, A. K., Spadoni, F., Stekhanov, V., Sun, X. L., Thibado, S., Tidball, A., Totev, T., Triambak, S., Tsang, T., Tyuka, O. A., van Bruggen, E., Vidal, M., Walent, M., Wamba, K., Wang, H. W., Wang, Q. D., Wang, W., Wang, Y. G., Watts, M., Wehrfritz, M., Wen, L. J., Wichoski, U., Wilde, S., Worcester, M., Xu, H., Yang, L., Yu, M., and Zeldovich, O.
Subjects: Physics - Atomic Physics, High Energy Physics - Experiment, Nuclear Experiment
Abstract: Neutrinoless double beta decay is one of the most sensitive probes for new physics beyond the Standard Model of particle physics. One of the isotopes under investigation is $^{136}$Xe, which would double beta decay into $^{136}$Ba. Detecting the single $^{136}$Ba daughter provides a sort of ultimate tool in the discrimination against backgrounds. Previous work demonstrated the ability to perform single atom imaging of Ba atoms in a single-vacancy site of a solid xenon matrix. In this paper, the effort to identify signal from individual barium atoms is extended to Ba atoms in a hexa-vacancy site in the matrix and is achieved despite increased photobleaching in this site. Abrupt fluorescence turn-off of a single Ba atom is also observed. Significant recovery of fluorescence signal lost through photobleaching is demonstrated upon annealing of Ba deposits in the Xe ice. Following annealing, it is observed that Ba atoms in the hexa-vacancy site exhibit antibleaching while Ba atoms in the tetra-vacancy site exhibit bleaching. This may be evidence for a matrix site transfer upon laser excitation. Our findings offer a path of continued research toward tagging of Ba daughters in all significant sites in solid xenon., Comment: 9 pages, 8 figures
Published: 2024

12. Decoupled static and dynamical charge correlations in La$_{2-x}$Sr$_x$CuO$_4$

Author: Martinelli, L., Biało, I., Hong, X., Oppliger, J., Lin, C., Schaller, T., Küspert, J., Fischer, M. H., Kurosawa, T., Momono, N., Oda, M., Choi, J., Agrestini, S., Garcia-Fernandez, M., Zhou, Ke-Jin, Wang, Q., and Chang, J.
Subjects: Condensed Matter - Strongly Correlated Electrons, Condensed Matter - Superconductivity
Abstract: The relation between charge order, its quantum fluctuations and optical phonon modes in cuprate superconductors remains an unsolved problem. The exploration of these excitations is however complicated by the presence of twinned domains. Here, we use uniaxial strain in combination with ultra-high-resolution Resonant Inelastic X-ray Scattering (RIXS) at the oxygen K- and copper L3-edges to study the excitations stemming from the charge ordering wave vector in La1.875Sr0.125CuO4. By detwinning stripe ordering, we demonstrate that the optical phonon anomalies do not show any stripe anisotropy. The low-energy charge excitations also retain an in-plane four-fold symmetry. As such, we find that both phonon and charge excitations are decoupled entirely from the strength of static charge ordering. The almost isotropic character of charge excitations remains a possible source for the strange metal properties found in the normal state of cuprate superconductors., Comment: 9 pages, 4 figures
Published: 2024

13. Multistructured accretion flow of Sgr A* II: Signatures of a Cool Accretion Disk in Hydrodynamic Simulations of Stellar Winds

Author: Balakrishnan, Mayura, Russell, Christopher M. P., Corrales, Lia, Calderón, Diego, Cuadra, Jorge, Haggard, Daryl, Markoff, Sera, Neilsen, Joey, Nowak, Michael, Wang, Q. Daniel, and Baganoff, Fred
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Hydrodynamic simulations of the stellar winds from Wolf-Rayet stars within the Galactic Center can provide predictions for the X-ray spectrum of supermassive black hole Sgr A*. Herein, we present results from updated smooth particle hydrodynamics simulations, building on the architecture of Cuadra et al. (2015); Russell et al. (2017), finding that a cold gas disk forms around Sgr A* with a simulation runtime of 3500 years. This result is consistent with previous grid-based simulations, demonstrating that a cold disk can form regardless of numerical method. We examine the plasma scenarios arising from an environment with and without this cold disk, by generating synthetic spectra for comparison to the quiescent Fe K alpha Sgr A* spectrum from Chandra HETG-S, taken through the Chandra X-ray Visionary Program. We find that current and future X-ray missions are unlikely to distinguish between the kinematic signatures in the plasma in these two scenarios. Nonetheless, the stellar wind plasma model presents a good fit to the dispersed Chandra spectra within 1.5" of Sgr A*. We compare our results to the Radiatively Inefficient Accretion Flow (RIAF) model fit to the HETG-S spectrum presented in Paper I and find that the Bayesian model evidence does not strongly favor either model. With 9" angular resolution and high spectral resolution of the X-IFU, NewAthena will offer a clearer differentiation between the RIAF plasma model and hydrodynamic simulations, but only a future X-ray mission with arcsecond resolution will significantly advance our understanding of Sgr A*'s accretion flow in X-rays., Comment: 14 pages, 6 figures. Accepted for publication in ApJ
Published: 2024

14. Multistructured accretion flow of Sgr A* I: Examination of a RIAF model

Author: Balakrishnan, Mayura, Corrales, Lia, Markoff, Sera, Nowak, Michael, Haggard, Daryl, Wang, Q. Daniel, Neilsen, Joey, Russell, Christopher M. P., Calderón, Diego, Cuadra, Jorge, and Baganoff, Fred
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: The extreme low-luminosity supermassive black hole Sgr A* provides a unique laboratory in which to test radiatively inefficient accretion flow (RIAF) models. Previous fits to the quiescent Chandra ACIS-S spectrum found a RIAF model with an equal inflow-outflow balance works well. In this work, we apply the RIAF model to the Chandra HETG-S spectrum obtained through the Chandra X-ray Visionary Program, which displays features suggestive of temperature and velocity structures within the plasma. A comprehensive forward model analysis accounting for the accretion flow geometry and HETG-S instrumental effects is required for a full interpretation of the quiescent Chandra HETG-S spectrum. We present a RIAF model that takes these effects into account. Our fits to the high-resolution gratings spectrum indicate an inflow balanced by an outflow ($s \sim 1$) alongside a temperature profile that appears shallower than what would be expected from a gravitational potential following $1/r$. The data require that the abundance of Iron relative to solar is $Z_{Fe} < 0.32 Z_\odot$ (90\% credible interval), much lower than the $2~Z_\odot$ metallicity measured in nearby late-type giants. While future missions like NewAthena will provide higher spectral resolution, source separation will continue to be a problem. Leveraging Chandra's unparalleled spatial resolution, which is not expected to be surpassed for decades, remains essential for detailed investigations of the densely populated Galactic Center in X-rays., Comment: 11 pages, 5 figures, 1 table. Accepted for publication in ApJ
Published: 2024

15. The coupling mechanism between crossed-beams energy transfer and stimulated Brillouin scattering in homogeneous plasmas

Author: Chen, Y., Wang, Q., Zheng, C. Y., Liu, Z. J., Cao, L. H., and Xiao, C. Z.
Subjects: Physics - Plasma Physics, Physics - Computational Physics
Abstract: The coupling mechanism between crossed beams energy transfer and stimulated Brillouin scattering in homogeneous plasmas are studied by theoretical analysis, fluid simulations and particle in cell(PIC) simulations. The numerical models of laser plasma instabilities are constructed by solving coupling equations with Schodinger equations form, and the fluid simulation results are confirmed by fluid theory and PIC simulations.In the parameter regime when the pump depletion does not occur in CBET and the reflectivity of SBS is lower than 1%, SBS will be affected by CBET, the CBET energy gain will still agree with theoretical predications. However, In the parameter regime when the pump depletion does occur in CBET and the reflectivity of SBS is higher than 1%, the CBET spatial gain will be reduced by the interaction of CBET and SBS, and the huge difference of SBS reflectivity for two crossed laser beams is observed.In the PIC simulations, we found that lower ZTe=Ti will significantly reduce the interaction between CBET and SBS (Z is the ion charge, Teis the electron temperature, Ti is the ion temperature)., Comment: 10pages,11 figures
Published: 2024

16. Discovery of An Apparent Red, High-Velocity Type Ia Supernova at z = 2.9 with JWST

Author: Pierel, J. D. R., Engesser, M., Coulter, D. A., Decoursey, C., Siebert, M. R., Rest, A., Egami, E., Chen, W., Fox, O. D., Jones, D. O., Joshi, B. A., Moriya, T. J., Zenati, Y., Bunker, A. J., Cargile, P. A., Curti, M., Eisenstein, D. J., Gezari, S., Gomez, S., Guolo, M., Johnson, B. D., Karmen, M., Maiolino, R., Quimby, Robert M., Robertson, B., Shahbandeh, M., Strolger, L. G., Sun, F., Wang, Q., and Wevers, T.
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: We present the JWST discovery of SN 2023adsy, a transient object located in a host galaxy JADES-GS$+53.13485$$-$$27.82088$ with a host spectroscopic redshift of $2.903\pm0.007$. The transient was identified in deep James Webb Space Telescope (JWST)/NIRCam imaging from the JWST Advanced Deep Extragalactic Survey (JADES) program. Photometric and spectroscopic followup with NIRCam and NIRSpec, respectively, confirm the redshift and yield UV-NIR light-curve, NIR color, and spectroscopic information all consistent with a Type Ia classification. Despite its classification as a likely SN Ia, SN 2023adsy is both fairly red (E(B-V)$\sim0.9$) despite a host galaxy with low-extinction and has a high Ca II velocity ($19,000\pm2,000$km/s) compared to the general population of SNe Ia. While these characteristics are consistent with some Ca-rich SNe Ia, particularly SN 2016hnk, SN 2023adsy is intrinsically brighter than the low-z Ca-rich population. Although such an object is too red for any low-z cosmological sample, we apply a fiducial standardization approach to SN 2023adsy and find that the SN 2023adsy luminosity distance measurement is in excellent agreement ($\lesssim1\sigma$) with $\Lambda$CDM. Therefore unlike low-z Ca-rich SNe Ia, SN 2023adsy is standardizable and gives no indication that SN Ia standardized luminosities change significantly with redshift. A larger sample of distant SNe Ia is required to determine if SN Ia population characteristics at high-z truly diverge from their low-z counterparts, and to confirm that standardized luminosities nevertheless remain constant with redshift., Comment: Submitted to ApJL
Published: 2024

17. Discovery of a Relativistic Stripped Envelope Type Ic-BL Supernova at z = 2.83 with JWST

Author: Siebert, M. R., Decoursey, C., Coulter, D. A., Engesser, M., Pierel, J. D. R., Rest, A., Egami, E., Shahbandeh, M., Chen, W., Fox, O. D., Zenati, Y., Moriya, T. J., Bunker, A. J., Cargile, P. A., Curti, M., Eisenstein, D. J., Gezari, S., Gomez, S., Guolo, M., Johnson, B. D., Joshi, B. A., Karmen, M., Maiolino, R., Quimby, R. M., Robertson, B., Strolger, L. G., Sun, F., Wang, Q., and Wevers, T.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We present JWST NIRCam and NIRSpec observations of a Type Ic supernova (SN Ic) and its host galaxy (JADES-GS+53.13533-27.81457) at $z = 2.83$. This SN (named SN 2023adta) was identified in deep James Webb Space Telescope (JWST)/NIRCam imaging from the JWST Advanced Deep Extragalactic Survey (JADES) Program. Follow-up observations with JWST/NIRSpec provided a spectroscopic redshift of $z = 2.83$ and the classification as a SN Ic-BL. The light curve of SN 2023adta matches well with other stripped envelope supernovae and we find a high peak luminosity, $M_V = -19.0 \pm 0.2$ mag, based on the distribution of best-fit SNe. The broad absorption features in its spectrum are consistent with other SNe Ic-BL 1-3 weeks after peak brightness. We measure a Ca II NIR triplet expansion velocity of $29{,}000 \pm 2{,}000$ km s$^{-1}$. The host galaxy of SN 2023adta is irregular, and modeling of its spectral energy distribution (SED) indicates a metallicity of $Z = 0.35^{+0.16}_{-0.08} Z_{\odot}$. This environment is consistent with the population of low-$z$ SNe Ic-BL which prefer lower metallicities relative to other stripped envelope supernovae, and track long duration $\gamma$-ray burst (LGRB) environments. We do not identify any GRBs that are coincident with SN 2023adta. Given the rarity of SNe Ic-BL in the local universe, the detection of a SN Ic-BL at $z = 2.83$ could indicate that their rates are enhanced at high redshift., Comment: 16 pages, 7 figures, Published in ApJL
Published: 2024

18. Supernova Electron-Neutrino Interactions with Xenon in the nEXO Detector

Author: nEXO Collaboration, Hedges, S., Kharusi, S. Al, Angelico, E., Brodsky, J. P., Richardson, G., Wilde, S., Amy, A., Anker, A., Arnquist, I. J., Arsenault, P., Atencio, A., Badhrees, I., Bane, J., Belov, V., Bernard, E. P., Bhatta, T., Bolotnikov, A., Breslin, J., Breur, P. A., Brown, E., Brunner, T., Caden, E., Cao, G. F., Cao, L. Q., Cesmecioglu, D., Chambers, E., Chana, B., Charlebois, S. A., Chernyak, D., Chiu, M., Collister, R., Cvitan, M., Dalmasson, J., Daniels, T., Darroch, L., DeVoe, R., di Vacri, M. L., Ding, Y. Y., Dolinski, M. J., Eckert, B., Elbeltagi, M., Elmansali, R., Fabris, L., Fairbank, W., Farine, J., Fatemighomi, N., Foust, B., Fu, Y. S., Gallacher, D., Gallice, N., Gillis, W., Goeldi, D., Gorham, A., Gornea, R., Gratta, G., Guan, Y. D., Hardy, C. A., Heffner, M., Hein, E., Holt, J. D., Hoppe, E. W., House, A., Hunt, W., Iverson, A., Kachru, P., Karelin, A., Keblbeck, D., Kuchenkov, A., Kumar, K. S., Larson, A., Latif, M. B., Leach, K. G., Lenardo, B. G., Leonard, D. S., Lewis, H., Li, G., Li, Z., Licciardi, C., Lindsay, R., MacLellan, R., Majidi, S., Malbrunot, C., Martel-Dion, P., Masbou, J., McMichael, K., Medina-Peregrina, M., Mong, B., Moore, D. C., Nattress, J., Natzke, C. R., Ngwadla, X. E., Ni, K., Nolan, A., Nowicki, S. C., Ondze, J. C. Nzobadila, Orrell, J. L., Ortega, G. S., Overman, C. T., Pagani, L., Smalley, H. Peltz, Perna, A., Piepke, A., Franco, T. Pinto, Pocar, A., Pratte, J. -F., Rasiwala, H., Ray, D., Raymond, K., Rescia, S., Riot, V., Ross, R., Saldanha, R., Sangiorgio, S., Schwartz, S., Sekula, S., Soderstrom, J., Soma, A. K., Spadoni, F., Sun, X. L., Thibado, S., Tidball, A., Totev, T., Triambak, S., Tsang, R. H. M., Tyuka, O. A., van Bruggen, E., Vidal, M., Viel, S., Walent, M., Wang, Q. D., Wang, W., Wang, Y. G., Watts, M., Wehrfritz, M., Wei, W., Wen, L. J., Wichoski, U., Wu, X. M., Xu, H., Yang, H. B., Yang, L., Yu, M., Yvaine, M., Zeldovich, O., and Zhao, J.
Subjects: High Energy Physics - Phenomenology, High Energy Physics - Experiment, Nuclear Theory
Abstract: Electron-neutrino charged-current interactions with xenon nuclei were modeled in the nEXO neutrinoless double-beta decay detector (~5-tonne, 90% ${}^{136}$Xe, 10% ${}^{134}$Xe) to evaluate its sensitivity to supernova neutrinos. Predictions for event rates and detectable signatures were modeled using the MARLEY event generator. We find good agreement between MARLEY's predictions and existing theoretical calculations of the inclusive cross sections at supernova neutrino energies. The interactions modeled by MARLEY were simulated within the nEXO simulation framework and were run through an example reconstruction algorithm to determine the detector's efficiency for reconstructing these events. The simulated data, incorporating the detector response, were used to study the ability of nEXO to reconstruct the incident electron-neutrino spectrum and these results were extended to a larger xenon detector of the same isotope enrichment. We estimate that nEXO will be able to observe electron-neutrino interactions with xenon from supernovae as far as 5 to 8 kpc from earth, while the ability to reconstruct incident electron-neutrino spectrum parameters from observed interactions in nEXO is limited to closer supernovae., Comment: 17 pages, 16 figures
Published: 2024

19. Search for solar axions by Primakoff effect with the full dataset of the CDEX-1B Experiment

Author: Yang, L. T., Liu, S. K., Yue, Q., Kang, K. J., Li, Y. J., An, H. P., C., Greeshma, Chang, J. P., Chen, Y. H., Cheng, J. P., Dai, W. H., Deng, Z., Fang, C. H., Geng, X. P., Gong, H., Guo, Q. J., Guo, T., Guo, X. Y., He, L., He, J. R., Hu, J. W., Huang, H. X., Huang, T. C., Jiang, L., Karmakar, S., Li, H. B., Li, H. Y., Li, J. M., Li, J., Li, M. C., Li, Q. Y., Li, R. M. J., Li, X. Q., Li, Y. L., Liang, Y. F., Liao, B., Lin, F. K., Lin, S. T., Liu, J. X., Liu, Y. D., Liu, Y., Liu, Y. Y., Ma, H., Mao, Y. C., Nie, Q. Y., Pan, H., Qi, N. C., Ren, J., Ruan, X. C., Shen, M. B., Singh, M. K., Sun, T. X., Sun, W. L., Tang, C. J., Tian, Y., Wang, G. F., Wang, J. Z., Wang, L., Wang, Q., Wang, Y. F., Wang, Y. X., Wong, H. T., Wu, Y. C., Xing, H. Y., Xiong, K. Z., Xu, R., Xu, Y., Xue, T., Yan, Y. L., Yi, N., Yu, C. X., Yu, H. J., Zeng, M., Zeng, Z., Zhang, B. T., Zhang, F. S., Zhang, L., Zhang, P., Zhang, Z. H., Zhang, Z. Y., Zhao, J. Z., Zhao, K. K., Zhao, M. G., Zhou, J. F., Zhou, Z. Y., and Zhu, J. J.
Subjects: High Energy Physics - Experiment, High Energy Physics - Phenomenology, Physics - Instrumentation and Detectors
Abstract: We present the first limit on $g_{A\gamma}$ coupling constant using the Bragg-Primakoff conversion based on an exposure of 1107.5 kg days of data from the CDEX-1B experiment at the China Jinping Underground Laboratory. The data are consistent with the null signal hypothesis, and no excess signals are observed. Limits of the coupling $g_{A\gamma}<2.08\times10^{-9}$ GeV$^{-1}$ (95\% C.L.) are derived for axions with mass up to 100 eV/$c^2$. Within the hadronic model of KSVZ, our results exclude axion mass $>5.3~\rm{eV}/c^2$ at 95\% C.L., Comment: 7 pages, 5 figures
Published: 2024

20. ATClean: A Novel Method for Detecting Low-Luminosity Transients and Application to Pre-explosion Counterparts from SN 2023ixf

Author: Rest, S., Rest, A., Kilpatrick, C. D., Jencson, J. E., von Coelln, S., Strolger, L., Smartt, S., Anderson, J. P., Clocchiatti, A., Coulter, D. A., Denneau, L., Gomez, S., Heinze, A., Ridden-Harper, R., Smith, K. W., Stalder, B., Tonry, J. l., Wang, Q., and Zenati, Y.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: In an effort to search for faint sources of emission over arbitrary timescales, we present a novel method for analyzing forced photometry light curves in difference imaging from optical surveys. Our method "ATLAS Clean'' or ATClean, utilizes the reported fluxes, uncertainties, and fits to the point-spread function from difference images to quantify the statistical significance of individual measurements. We apply this method to control light curves across the image to determine whether any source of flux is present in the data for a range of specific timescales. From ATLAS $o$-band imaging at the site of the Type II supernova (SN) 2023ixf in M101 from 2015--2023, we show that this method accurately reproduces the 3$\sigma$ flux limits produced from other, more computationally expensive methods. We derive limits for emission on timescales of 5~days and 80-300~days at the site of SN\,2023ixf, which are 19.8 and 21.3~mag, respectively. The latter limits rule out variability for unextinguished red supergiants (RSG) with initial masses $>$22~$M_{\odot}$, comparable to the most luminous predictions for the SN 2023ixf progenitor system. We also compare our limits to short timescale outbursts, similar to those expected for Type IIn SN progenitor stars or the Type II SN 2020tlf, and rule out outburst ejecta masses of $>$0.021~$M_{\odot}$, much lower than the inferred mass of circumstellar matter around SN 2023ixf in the literature. In the future, these methods can be applied to any forced point-spread function photometry on difference imaging from other surveys, such as Rubin optical imaging., Comment: 24 pages, 19 figures
Published: 2024

21. Discovery of Giant Unit-Cell Super-Structure in the Infinite-Layer Nickelate PrNiO$_2$

Author: Oppliger, J., Küspert, J., Dippel, A. -C., Zimmermann, M. v., Gutowski, O., Ren, X., Zhou, X. J., Zhu, Z., Frison, R., Wang, Q., Martinelli, L., Biało, I., and Chang, J.
Subjects: Condensed Matter - Superconductivity, Condensed Matter - Materials Science
Abstract: Spectacular quantum phenomena such as superconductivity often emerge in flat-band systems where Coulomb interactions overpower electron kinetics. Engineering strategies for flat-band physics is therefore of great importance. Here, using high-energy grazing-incidence x-ray diffraction, we demonstrate how in-situ temperature annealing of the infinite-layer nickelate PrNiO$_2$ induces a giant superlattice structure. The annealing effect has a maximum well above room temperature. By covering a large scattering volume, we show a rare period-six in-plane (bi-axial) symmetry and a period-four symmetry in the out-of-plane direction. This giant unit-cell superstructure likely stems from ordering of diffusive oxygen. The stability of this superlattice structure suggests a connection to an energetically favorable electronic state of matter. As such, our study provides a new pathway - different from Moir\'e structures - to ultra-small Brillouin zone electronics., Comment: Main: 7 pages, 4 figures. Supplementary: 2 pages, 3 figures
Published: 2024

22. First Search for Light Fermionic Dark Matter Absorption on Electrons Using Germanium Detector in CDEX-10 Experiment

Author: Liu, J. X., Yang, L. T., Yue, Q., Kang, K. J., Li, Y. J., An, H. P., C., Greeshma, Chang, J. P., Chen, Y. H., Cheng, J. P., Dai, W. H., Deng, Z., Fang, C. H., Geng, X. P., Gong, H., Guo, Q. J., Guo, T., Guo, X. Y., He, L., He, J. R., Hu, J. W., Huang, H. X., Huang, T. C., Jiang, L., Karmakar, S., Li, H. B., Li, H. Y., Li, J. M., Li, J., Li, M. C., Li, Q. Y., Li, R. M. J., Li, X. Q., Li, Y. L., Liang, Y. F., Liao, B., Lin, F. K., Lin, S. T., Liu, S. K., Liu, Y. D., Liu, Y., Liu, Y. Y., Ma, H., Mao, Y. C., Nie, Q. Y., Pan, H., Qi, N. C., Ren, J., Ruan, X. C., Shen, M. B., Singh, M. K., Sun, T. X., Sun, W. L., Tang, C. J., Tian, Y., Wang, G. F., Wang, J. Z., Wang, L., Wang, Q., Wang, Y. F., Wang, Y. X., Wong, H. T., Wu, Y. C., Xing, H. Y., Xiong, K. Z., Xu, R., Xu, Y., Xue, T., Yan, Y. L., Yi, N., Yu, C. X., Yu, H. J., Zeng, M., Zeng, Z., Zhang, B. T., Zhang, F. S., Zhang, L., Zhang, P., Zhang, Z. H., Zhang, Z. Y., Zhao, J. Z., Zhao, K. K., Zhao, M. G., Zhou, J. F., Zhou, Z. Y., and Zhu, J. J.
Subjects: High Energy Physics - Experiment, High Energy Physics - Phenomenology, Physics - Instrumentation and Detectors
Abstract: We present the first results of the search for sub-MeV fermionic dark matter absorbed by electron targets of Germanium using the 205.4~kg$\cdot$day data collected by the CDEX-10 experiment, with the analysis threshold of 160~eVee. No significant dark matter (DM) signals over the background are observed. Results are presented as limits on the cross section of DM--electron interaction. We present new constraints of cross section in the DM range of 0.1--10 keV/$c^2$ for vector and axial-vector interaction. The upper limit on the cross section is set to be $\rm 5.5\times10^{-46}~cm^2$ for vector interaction, and $\rm 1.8\times10^{-46}~cm^2$ for axial-vector interaction at DM mass of 5 keV/$c^2$., Comment: 6 pages, 4 figures
Published: 2024

23. FEASTS Combined with Interferometry (I): Overall Properties of Diffuse HI and Implications for Gas Accretion in Nearby Galaxies

Author: Wang, Jing, Lin, Xuchen, Yang, Dong, Staveley-Smith, Lister, Walter, Fabian, Wang, Q. Daniel, Wang, Ran, Battisti, A. J., Catinella, Barbara, Chen, Hsiao-Wen, Cortese, Luca, Fisher, D. B., Ho, Luis C., Ji, Suoqing, Jiang, Peng, Kauffmann, Guinevere, Kong, Xu, Liu, Ziming, Shao, Li, Wang, Jie, Wang, Lile, and Wang, Shun
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We present a statistical study of the properties of diffuse HI in ten nearby galaxies, comparing the HI detected by the single-dish telescope FAST (FEASTS program) and the interferometer VLA (THINGS program), respectively. The THINGS' observation missed HI with a median of 23% due to the short-spacing problem of interferometry and limited sensitivity. We extract the diffuse HI by subtracting the dense HI, which is obtained from the THINGS data with a uniform flux-density threshold, from the total HI detected by FAST. Among the sample, the median diffuse-HI fraction is 34%, and more diffuse HI is found in galaxies exhibiting more prominent tidal-interaction signatures. The diffuse HI we detected seems to be distributed in disk-like layers within a typical thickness of $1\,\text{kpc}$, different from the more halo-like diffuse HI detected around NGC 4631 in a previous study. Most of the diffuse HI is cospatial with the dense HI and has a typical column density of $10^{17.7}$-$10^{20.1}\,\text{cm}^{-2}$. The diffuse and dense HI exhibits a similar rotational motion, but the former lags by a median of 25% in at least the inner disks, and its velocity dispersions are typically twice as high. Based on a simplified estimation of circum-galactic medium properties and assuming pressure equilibrium, the volume density of diffuse HI appears to be constant within each individual galaxy, implying its role as a cooling interface. Comparing with existing models, these results are consistent with a possible link between tidal interactions, the formation of diffuse HI, and gas accretion., Comment: 45 pages, 23 figures. In press at ApJ. Data will be released at the FEASTS site upon publication
Published: 2024

24. Birds of a Feather: Resolving Stellar Mass Assembly With JWST/NIRCam in a Pair of Kindred $z \sim 2$ Dusty Star-forming Galaxies Lensed by the PLCK G165.7+67.0 Cluster

Author: Kamieneski, Patrick S., Frye, Brenda L., Windhorst, Rogier A., Harrington, Kevin C., Yun, Min S., Noble, Allison, Pascale, Massimo, Foo, Nicholas, Cohen, Seth H., Jansen, Rolf A., Carleton, Timothy, Koekemoer, Anton M., Willmer, Christopher N. A., Summers, Jake S., Garuda, Nikhil, Leimbach, Reagen, Holwerda, Benne W., Pierel, Justin D. R., Jimenez-Andrade, Eric F., Willner, S. P., Pampliega, Belen Alcalde, Vishwas, Amit, Keel, William C., Wang, Q. Daniel, Cheng, Cheng, Coe, Dan, Conselice, Christopher J., D'Silva, Jordan C. J., Driver, Simon P., Grogin, Norman A., Hinrichs, Tyler, Lowenthal, James D., Marshall, Madeline A., Nonino, Mario, Ortiz III, Rafael, Pigarelli, Alex, Pirzkal, Nor, Polletta, Maria del Carmen, Robotham, Aaron S. G., Ryan Jr., Russell E., and Yan, Haojing
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We present a new parametric lens model for the G165.7+67.0 galaxy cluster, which was discovered with $Planck$ through its bright submillimeter flux, originating from a pair of extraordinary dusty star-forming galaxies (DSFGs) at $z\approx 2.2$. Using JWST and interferometric mm/radio observations, we characterize the intrinsic physical properties of the DSFGs, which are separated by only $\sim 1^{\prime\prime}$ (8 kpc) and a velocity difference $\Delta V \lesssim 600~{\rm km}~{\rm s}^{-1}$ in the source plane, and thus likely undergoing a major merger. Boasting intrinsic star formation rates ${\rm SFR}_{\rm IR} = 320 \pm 70$ and $400 \pm 80~ M_\odot~{\rm yr}^{-1}$, stellar masses ${\rm log}[M_\star/M_\odot] = 10.2 \pm 0.1$ and $10.3 \pm 0.1$, and dust attenuations $A_V = 1.5 \pm 0.3$ and $1.2 \pm 0.3$, they are remarkably similar objects. We perform spatially-resolved pixel-by-pixel SED fitting using rest-frame near-UV to near-IR imaging from JWST/NIRCam for both galaxies, resolving some stellar structures down to 100 pc scales. Based on their resolved specific SFRs and $UVJ$ colors, both DSFGs are experiencing significant galaxy-scale star formation events. If they are indeed interacting gravitationally, this strong starburst could be the hallmark of gas that has been disrupted by an initial close passage. In contrast, the host galaxy of the recently discovered triply-imaged SN H0pe has a much lower SFR than the DSFGs, and we present evidence for the onset of inside-out quenching and large column densities of dust even in regions of low specific SFR. Based on the intrinsic SFRs of the DSFGs inferred from UV through FIR SED modeling, this pair of objects alone is predicted to yield an observable $1.1 \pm 0.2~{\rm CCSNe~yr}^{-1}$, making this cluster field ripe for continued monitoring., Comment: 47 pages, 21 figures, 5 tables. Submitted to ApJ, comments welcome!
Published: 2024

25. A broad linewidth, compact, millimeter-bright molecular emission line source near the Galactic Center

Author: Ginsburg, Adam, Bally, John, Barnes, Ashley T., Battersby, Cara, Budaiev, Nazar, Butterfield, Natalie O., Caselli, Paola, Colzi, Laura, Dutkowska, Katarzyna M., García, Pablo, Gramze, Savannah, Henshaw, Jonathan D., Hu, Yue, Jeff, Desmond, Jiménez-Serra, Izaskun, Kauffmann, Jens, Klessen, Ralf S., Levesque, Emily M., Longmore, Steven N., Lu, Xing, Mills, Elisabeth A. C., Morris, Mark R., Nogueras-Lara, Francisco, Oka, Tomoharu, Pineda, Jaime E., Pillai, Thushara G. S., Rivilla, Víctor M., Sánchez-Monge, Álvaro, Santa-Maria, Miriam G., Smith, Howard A., Sofue, Yoshiaki, Sormani, Mattia C., Tremblay, Grant R., Vermariën, Gijs, Vikhlinin, Alexey, Viti, Serena, Walker, Dan, Wang, Q. Daniel, Xu, Fengwei, and Zhang, Qizhou
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: A compact source, G0.02467-0.0727, was detected in ALMA \threemm observations in continuum and very broad line emission. The continuum emission has a spectral index $\alpha\approx3.3$, suggesting that the emission is from dust. The line emission is detected in several transitions of CS, SO, and SO$_2$ and exhibits a line width FWHM $\approx160$ \kms. The line profile appears Gaussian. The emission is weakly spatially resolved, coming from an area on the sky $\lesssim1"$ in diameter ($\lesssim10^4$ AU at the distance of the Galactic Center; GC). The centroid velocity is $v_{LSR}\approx40$-$50$ \kms, which is consistent with a location in the Galactic Center. With multiple SO lines detected, and assuming local thermodynamic equilibrium (LTE) conditions, $T_\mathrm{LTE} = 13$ K, which is colder than seen in typical GC clouds, though we cannot rule out low-density, subthermally excited, warmer gas. Despite the high velocity dispersion, no emission is observed from SiO, suggesting that there are no strong ($\gtrsim10~\mathrm{km~s}^{-1}$) shocks in the molecular gas. There are no detections at other wavelengths, including X-ray, infrared, and radio. We consider several explanations for the Millimeter Ultra-Broad Line Object (MUBLO), including protostellar outflow, explosive outflow, collapsing cloud, evolved star, stellar merger, high-velocity compact cloud, intermediate mass black hole, and background galaxy. Most of these conceptual models are either inconsistent with the data or do not fully explain it. The MUBLO is, at present, an observationally unique object., Comment: Accepted to ApJL
Published: 2024

26. eDIG-CHANGES II: Project Design and Initial Results on NGC 3556

Author: Li, Jiang-Tao, Lu, Li-Yuan, Qu, Zhijie, Benjamin, Robert A., Bregman, Joel N., Dettmar, Ralf-Jurgen, English, Jayanne, Fang, Taotao, Irwin, Judith A., Jiang, Yan, Li, Hui, Liu, Guilin, Martini, Paul, Rand, Richard J., Stein, Yelena, Strong, Andrew W., Vargas, Carlos J., Wang, Q. Daniel, Wang, Jing, Wiegert, Theresa, Xu, Jianghui, and Yang, Yang
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena
Abstract: The extraplanar diffuse ionized gas (eDIG) represents ionized gases traced by optical/UV lines beyond the stellar extent of galaxies. We herein introduce a novel multi-slit narrow-band spectroscopy method to conduct spatially resolved spectroscopy of the eDIG around a sample of nearby edge-on disk galaxies (eDIG-CHANGES). In this paper, we introduce the project design and major scientific goals, as well as a pilot study of NGC 3556 (M108). The eDIG is detected to a vertical extent of a few kpc above the disk, comparable to the X-ray and radio images. We do not see significant vertical variation of the [N II]/H$\alpha$ line ratio. A rough examination of the pressure balance between different circum-galactic medium (CGM) phases indicates the magnetic field is in a rough pressure balance with the X-ray emitting hot gas, and may play an important role in the global motion of both the eDIG and the hot gas in the lower halo. At the location of an HST/COS observed UV bright background AGN $\sim29\rm~kpc$ from the center of NGC 3556, the magnetic pressure is much lower than that of the hot gas and the ionized gas traced by UV absorption lines, although the extrapolation of the pressure profiles may cause some biases in this comparison. By comparing the position-velocity diagrams of the optical and CO lines, we also find the dynamics of the two gas phases are consistent with each other, with no evidence of a global inflow/outflow and a maximum rotation velocity of $\sim150\rm~km~s^{-1}$., Comment: 19 pages, 9 figures, 1 table, accepted for publication in ApJ
Published: 2024

27. Lensed Type Ia Supernova 'Encore' at z=2: The First Instance of Two Multiply-Imaged Supernovae in the Same Host Galaxy

Author: Pierel, J. D. R., Newman, A. B., Dhawan, S., Gu, M., Joshi, B. A., Li, T., Schuldt, S., Strolger, L. G., Suyu, S. H., Caminha, G. B., Cohen, S. H., Diego, J. M., Dsilva, J. C. J., Ertl, S., Frye, B. L., Granata, G., Grillo, C., Koekemoer, A. M., Li, J., Robotham, A., Summers, J., Treu, T., Windhorst, R. A., Zitrin, A., Agarwal, S., Agrawal, A., Arendse, N., Belli, S., Burns, C., Cañameras, R., Chakrabarti, S., Chen, W., Collett, T. E., Coulter, D. A., Ellis, R. S., Engesser, M., Foo, N., Fox, O. D., Gall, C., Garuda, N., Gezari, S., Gomez, S., Glazebrook, K., Hjorth, J., Huang, X., Jha, S. W., Kamieneski, P. S., Kelly, P., Larison, C., Moustakas, L. A., Pascale, M., Pérez-Fournon, I., Petrushevska, T., Poidevin, F., Rest, A., Shahbandeh, M., Shajib, A. J., Siebert, M., Storfer, C., Talbot, M., Wang, Q., Wevers, T., and Zenati, Y.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: A bright ($m_{\rm F150W,AB}$=24 mag), $z=1.95$ supernova (SN) candidate was discovered in JWST/NIRCam imaging acquired on 2023 November 17. The SN is quintuply-imaged as a result of strong gravitational lensing by a foreground galaxy cluster, detected in three locations, and remarkably is the second lensed SN found in the same host galaxy. The previous lensed SN was called "Requiem", and therefore the new SN is named "Encore". This makes the MACS J0138.0$-$2155 cluster the first known system to produce more than one multiply-imaged SN. Moreover, both SN Requiem and SN Encore are Type Ia SNe (SNe Ia), making this the most distant case of a galaxy hosting two SNe Ia. Using parametric host fitting, we determine the probability of detecting two SNe Ia in this host galaxy over a $\sim10$ year window to be $\approx3\%$. These observations have the potential to yield a Hubble Constant ($H_0$) measurement with $\sim10\%$ precision, only the third lensed SN capable of such a result, using the three visible images of the SN. Both SN Requiem and SN Encore have a fourth image that is expected to appear within a few years of $\sim2030$, providing an unprecedented baseline for time-delay cosmography., Comment: Accepted, ApJL
Published: 2024
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28. Constraints on the Blazar-Boosted Dark Matter from the CDEX-10 Experiment

Author: Xu, R., Yang, L. T., Yue, Q., Kang, K. J., Li, Y. J., An, H. P., C., Greeshma, Chang, J. P., Chen, Y. H., Cheng, J. P., Dai, W. H., Deng, Z., Fang, C. H., Geng, X. P., Gong, H., Guo, Q. J., Guo, T., Guo, X. Y., He, L., He, S. M., Hu, J. W., Huang, H. X., Huang, T. C., Jiang, L., Karmakar, S., Li, H. B., Li, H. Y., Li, J. M., Li, J., Li, Q. Y., Li, R. M. J., Li, X. Q., Li, Y. L., Liang, Y. F., Liao, B., Lin, F. K., Lin, S. T., Liu, J. X., Liu, S. K., Liu, Y. D., Liu, Y., Liu, Y. Y., Ma, H., Mao, Y. C., Nie, Q. Y., Ning, J. H., Pan, H., Qi, N. C., Ren, J., Ruan, X. C., Singh, M. K., Sun, T. X., Tang, C. J., Tian, Y., Wang, G. F., Wang, J. Z., Wang, L., Wang, Q., Wang, Y. F., Wang, Y. X., Wong, H. T., Wu, S. Y., Wu, Y. C., Xing, H. Y., Xu, Y., Xue, T., Yan, Y. L., Yi, N., Yu, C. X., Yu, H. J., Yue, J. F., Zeng, M., Zeng, Z., Zhang, B. T., Zhang, F. S., Zhang, L., Zhang, Z. H., Zhang, Z. Y., Zhao, J. Z., Zhao, K. K., Zhao, M. G., Zhou, J. F., Zhou, Z. Y., and Zhu, J. J.
Subjects: High Energy Physics - Experiment, High Energy Physics - Phenomenology, Physics - Instrumentation and Detectors
Abstract: We report new constraints on light dark matter (DM) boosted by blazars using the 205.4 kg day data from the CDEX-10 experiment located at the China Jinping Underground Laboratory. Two representative blazars, TXS 0506+56 and BL Lacertae are studied. The results derived from TXS 0506+56 exclude DM-nucleon elastic scattering cross sections from $4.6\times 10^{-33}\ \rm cm^2$ to $1\times10^{-26}\ \rm cm^2$ for DM masses between 10 keV and 1 GeV, and the results derived from BL Lacertae exclude DM-nucleon elastic scattering cross sections from $2.4\times 10^{-34}\ \rm cm^2$ to $1\times10^{-26}\ \rm cm^2$ for the same range of DM masses. The constraints correspond to the best sensitivities among solid-state detector experiments in the sub-MeV mass range., Comment: 7 pages, 4 figures
Published: 2024

29. Probing Dark Matter Particles from Evaporating Primordial Black Holes via Electron Scattering in the CDEX-10 Experiment

Author: Zhang, Z. H., Yang, L. T., Yue, Q., Kang, K. J., Li, Y. J., An, H. P., C., Greeshma, Chang, J. P., Chen, Y. H., Cheng, J. P., Dai, W. H., Deng, Z., Fang, C. H., Geng, X. P., Gong, H., Guo, Q. J., Guo, T., Guo, X. Y., He, L., He, S. M., Hu, J. W., Huang, H. X., Huang, T. C., Jiang, L., Karmakar, S., Li, H. B., Li, H. Y., Li, J. M., Li, J., Li, Q. Y., Li, R. M. J., Li, X. Q., Li, Y. L., Liang, Y. F., Liao, B., Lin, F. K., Lin, S. T., Liu, J. X., Liu, S. K., Liu, Y. D., Liu, Y., Liu, Y. Y., Ma, H., Mao, Y. C., Nie, Q. Y., Ning, J. H., Pan, H., Qi, N. C., Ren, J., Ruan, X. C., Singh, M. K., Sun, T. X., Tang, C. J., Tian, Y., Wang, G. F., Wang, J. Z., Wang, L., Wang, Q., Wang, Y. F., Wang, Y. X., Wong, H. T., Wu, S. Y., Wu, Y. C., Xing, H. Y., Xu, R., Xu, Y., Xue, T., Yan, Y. L., Yi, N., Yu, C. X., Yu, H. J., Yue, J. F., Zeng, M., Zeng, Z., Zhang, B. T., Zhang, F. S., Zhang, L., Zhang, Z. Y., Zhao, J. Z., Zhao, K. K., Zhao, M. G., Zhou, J. F., Zhou, Z. Y., and Zhu, J. J.
Subjects: High Energy Physics - Experiment, High Energy Physics - Phenomenology, Physics - Instrumentation and Detectors
Abstract: Dark matter (DM) is a major constituent of the Universe. However, no definite evidence of DM particles (denoted as ``$\chi$") has been found in DM direct detection (DD) experiments to date. There is a novel concept of detecting $\chi$ from evaporating primordial black holes (PBHs). We search for $\chi$ emitted from PBHs by investigating their interaction with target electrons. The examined PBH masses range from 1$\times$10$^{15}$ to 7$\times$10$^{16}$ g under the current limits of PBH abundance $f_{PBH}$. Using 205.4 kg$\cdot$day data obtained from the CDEX-10 experiment conducted in the China Jinping Underground Laboratory, we exclude the $\chi$--electron ($\chi$--$e$) elastic-scattering cross section $\sigma_{\chi e} \sim 5\times10^{-29}$ cm$^2$ for $\chi$ with a mass $m_{\chi}\lesssim$ 0.1 keV from our results. With the higher radiation background but lower energy threshold (160 eV), CDEX-10 fill a part of the gap in the previous work. If ($m_{\chi}$, $\sigma_{\chi e}$) can be determined in the future, DD experiments are expected to impose strong constraints on $f_{PBH}$ for large $M_{PBH}$s., Comment: 9 pages, 6 figures, 3 tables. Version updated to match SCPMA version
Published: 2024
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30. CHANG-ES. XXX. 10 kpc Radio Lobes in The Sombrero Galaxy

Author: Yang, Yang, Li, Jiang-Tao, Wiegert, Theresa, Li, Zhiyuan, Guo, Fulai, Irwin, Judith, Wang, Q. Daniel, Dettmar, Ralf-Juergen, Beck, Rainer, English, Jayanne, and Ji, Li
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We report the discovery of the 10 kilo-parsec (kpc) scale radio lobes in the Sombrero galaxy (NGC 4594), using data from the Continuum Halos in Nearby Galaxies - an Expanded Very Large Array (VLA) Survey (CHANG-ES) project. We further examine the balance between the magnetic pressure inside the lobes and the thermal pressure of the ambient hot gas. At the radii $r$ of ~(1-10) kpc, the magnetic pressure inside the lobes and the thermal pressure of the ambient hot gas are generally in balance. This implies that the jets could expand into the surroundings at least to r ~ 10 kpc. The feedback from the active galactic nucleus (AGN) jet responsible for the large-scale lobes may help to explain the unusually high X-ray luminosity of this massive quiescent isolated disk galaxy, although more theoretical work is needed to further examine this possibility., Comment: 8 pages, 3 figures, 2 tables, accepted for publication in ApJ
Published: 2024

31. Non-Equilibrium and Self-Organization Evolution in Hot-Spot Ignition Processes

Author: Fu, X. -Y., Guo, Z. -Y., Wang, Q. -H., Wang, R. -C., Wu, D., and Zhang, J.
Subjects: Physics - Plasma Physics
Abstract: Due to disparate formation mechanisms, as for central hot-spot ignition and fast ignition, the initial temperatures of electron and ions usually differs from each other in the hot spot. Considering the percipient dependence of fusion cross-section and energy losses on temperature, this difference manifests the inadequacy of the equilibrium theoretical model in accurately depicting the ignition condition and evolution of the hot-spot. In this work, we studied a non-equilibrium model and extended this model to both isobaric and isochoric scenarios, characterized by varying hot-spot densities, temperatures and expansion velocities. In both cases, a spontaneous self-organization evolution was observed, manifesting as the bifurcation of ion and electron temperatures. Notably, the ion temperature is particularly prominent during the ignition process. This inevitability can be traced to the preponderant deposition rates of alpha-particles into D-T ions and the decreasing rate of energy exchange between electrons and D-T ions at elevated temperatures. The inherent structure, characterized by higher ion temperature and lower electron temperature during ignition, directly contributes to the augmentation of D-T reactions and mitigates energy losses through electron conduction and bremsstrahlung, thereby naturally facilitating nuclear fusions., Comment: The junior undergraduate students, X.-Y. Fu, Z.-Y. Guo, Q.-H. Wang, and R.-C. Wang, all contributed equally to this work
Published: 2024

32. Monitoring Microstructure and Properties Changes in 35CrMo Steel Components Using Magnetic Hysteresis Loop and X-Ray Diffraction Techniques

Author: Chen, H., Xu, B., Shen, Z.-X., Niu, Y.-P., Zhou, J., Zhu, J.-D., Cao, G.-M., and Wang, Q.
Published: 2024
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33. An Advanced Chemometric Model Applied to Ratiometric Surface-Enhanced Raman Scattering for Monitoring Blood Glucose

Author: Tang, Y., Zhang, S.-W., Wang, Q., Han, J.-J., Chao, L., Nie, L.-B., Chen, Y., and Wang, T.
Published: 2024
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34. Measurement of differential ZZ + jets production cross sections in pp collisions at s = 13 TeV

Author: Hayrapetyan, A., Tumasyan, A., Adam, W., Andrejkovic, J. W., Bergauer, T., Chatterjee, S., Damanakis, K., Dragicevic, M., Escalante Del Valle, A., Hussain, P. S., Jeitler, M., Krammer, N., Liko, D., Mikulec, I., Schieck, J., Schöfbeck, R., Schwarz, D., Sonawane, M., Templ, S., Waltenberger, W., Wulz, C.-E., Darwish, M. R., Janssen, T., Van Mechelen, P., Bols, E. S., D’Hondt, J., Dansana, S., De Moor, A., Delcourt, M., El Faham, H., Lowette, S., Makarenko, I., Müller, D., Sahasransu, A. R., Tavernier, S., Tytgat, M., Van Putte, S., Vannerom, D., Clerbaux, B., De Lentdecker, G., Favart, L., Hohov, D., Jaramillo, J., Khalilzadeh, A., Lee, K., Mahdavikhorrami, M., Malara, A., Paredes, S., Pétré, L., Postiau, N., Thomas, L., Vanden Bemden, M., Vander Velde, C., Vanlaer, P., De Coen, M., Dobur, D., Hong, Y., Knolle, J., Lambrecht, L., Mestdach, G., Rendón, C., Samalan, A., Skovpen, K., Van Den Bossche, N., Wezenbeek, L., Benecke, A., Bruno, G., Caputo, C., Delaere, C., Donertas, I. S., Giammanco, A., Jaffel, K., Jain, Sa., Lemaitre, V., Lidrych, J., Mastrapasqua, P., Mondal, K., Tran, T. T., Wertz, S., Alves, G. A., Coelho, E., Hensel, C., Menezes De Oliveira, T., Moraes, A., Rebello Teles, P., Soeiro, M., Aldá Júnior, W. L., Alves Gallo Pereira, M., Barroso Ferreira Filho, M., Brandao Malbouisson, H., Carvalho, W., Chinellato, J., Da Costa, E. M., Da Silveira, G. G., De Jesus Damiao, D., Fonseca De Souza, S., Martins, J., Mora Herrera, C., Mota Amarilo, K., Mundim, L., Nogima, H., Santoro, A., Silva Do Amaral, S. M., Sznajder, A., Thiel, M., Vilela Pereira, A., Bernardes, C. A., Calligaris, L., Fernandez Perez Tomei, T. R., Gregores, E. M., Mercadante, P. G., Novaes, S. F., Orzari, B., Padula, Sandra S., Aleksandrov, A., Antchev, G., Hadjiiska, R., Iaydjiev, P., Misheva, M., Shopova, M., Sultanov, G., Dimitrov, A., Ivanov, T., Litov, L., Pavlov, B., Petkov, P., Petrov, A., Shumka, E., Keshri, S., Thakur, S., Cheng, T., Guo, Q., Javaid, T., Mittal, M., Yuan, L., Bauer, G., Hu, Z., Liu, J., Yi, K., Chen, G. M., Chen, H. S., Chen, M., Iemmi, F., Jiang, C. H., Kapoor, A., Liao, H., Liu, Z.-A., Monti, F., Shahzad, M. A., Sharma, R., Song, J. N., Tao, J., Wang, C., Wang, J., Wang, Z., Zhang, H., Agapitos, A., Ban, Y., Levin, A., Li, C., Li, Q., Mao, Y., Qian, S. J., Sun, X., Wang, D., Yang, H., Zhang, L., Zhou, C., You, Z., Lu, N., Gao, X., Leggat, D., Okawa, H., Zhang, Y., Lin, Z., Lu, C., Xiao, M., Avila, C., Barbosa Trujillo, D. A., Cabrera, A., Florez, C., Fraga, J., Reyes Vega, J. A., Mejia Guisao, J., Ramirez, F., Rodriguez, M., Ruiz Alvarez, J. D., Giljanovic, D., Godinovic, N., Lelas, D., Sculac, A., Kovac, M., Sculac, T., Bargassa, P., Brigljevic, V., Chitroda, B. K., Ferencek, D., Mishra, S., Starodumov, A., Susa, T., Attikis, A., Christoforou, K., Konstantinou, S., Mousa, J., Nicolaou, C., Ptochos, F., Razis, P. A., Rykaczewski, H., Saka, H., Stepennov, A., Finger, M., Finger, Jr., M., Kveton, A., Ayala, E., Carrera Jarrin, E., Abdelalim, A. A., Salama, E., Mahmoud, M. A., Mohammed, Y., Dewanjee, R. K., Ehataht, K., Kadastik, M., Lange, T., Nandan, S., Nielsen, C., Pata, J., Raidal, M., Tani, L., Veelken, C., Kirschenmann, H., Osterberg, K., Voutilainen, M., Bharthuar, S., Brücken, E., Garcia, F., Havukainen, J., Kallonen, K. T. S., Kim, M. S., Kinnunen, R., Lampén, T., Lassila-Perini, K., Lehti, S., Lindén, T., Lotti, M., Martikainen, L., Myllymäki, M., Rantanen, M. m., Siikonen, H., Tuominen, E., Tuominiemi, J., Luukka, P., Petrow, H., Tuuva, T., Besancon, M., Couderc, F., Dejardin, M., Denegri, D., Faure, J. L., Ferri, F., Ganjour, S., Gras, P., Hamel de Monchenault, G., Lohezic, V., Malcles, J., Rander, J., Rosowsky, A., Sahin, M. Ö., Savoy-Navarro, A., Simkina, P., Titov, M., Baldenegro Barrera, C., Beaudette, F., Buchot Perraguin, A., Busson, P., Cappati, A., Charlot, C., Damas, F., Davignon, O., De Wit, A., Falmagne, G., Fontana Santos Alves, B. A., Ghosh, S., Gilbert, A., Granier de Cassagnac, R., Hakimi, A., Harikrishnan, B., Kalipoliti, L., Liu, G., Motta, J., Nguyen, M., Ochando, C., Portales, L., Salerno, R., Sarkar, U., Sauvan, J. B., Sirois, Y., Tarabini, A., Vernazza, E., Zabi, A., Zghiche, A., Agram, J.-L., Andrea, J., Apparu, D., Bloch, D., Brom, J.-M., Chabert, E. C., Collard, C., Falke, S., Goerlach, U., Grimault, C., Haeberle, R., Le Bihan, A.-C., Sessini, M. A., Van Hove, P., Beauceron, S., Blancon, B., Boudoul, G., Chanon, N., Choi, J., Contardo, D., Depasse, P., Dozen, C., El Mamouni, H., Fay, J., Gascon, S., Gouzevitch, M., Greenberg, C., Grenier, G., Ille, B., Laktineh, I. B., Lethuillier, M., Mirabito, L., Perries, S., Purohit, A., Vander Donckt, M., Verdier, P., Xiao, J., Lomidze, I., Toriashvili, T., Tsamalaidze, Z., Botta, V., Feld, L., Klein, K., Lipinski, M., Meuser, D., Pauls, A., Röwert, N., Teroerde, M., Diekmann, S., Dodonova, A., Eich, N., Eliseev, D., Engelke, F., Erdmann, M., Fackeldey, P., Fischer, B., Hebbeker, T., Hoepfner, K., Ivone, F., Jung, A., Lee, M. y., Mastrolorenzo, L., Merschmeyer, M., Meyer, A., Mukherjee, S., Noll, D., Novak, A., Nowotny, F., Pozdnyakov, A., Rath, Y., Redjeb, W., Rehm, F., Reithler, H., Sarkisovi, V., Schmidt, A., Schuler, S. C., Sharma, A., Stein, A., Torres Da Silva De Araujo, F., Vigilante, L., Wiedenbeck, S., Zaleski, S., Dziwok, C., Flügge, G., Haj Ahmad, W., Kress, T., Nowack, A., Pooth, O., Stahl, A., Ziemons, T., Zotz, A., Aarup Petersen, H., Aldaya Martin, M., Alimena, J., Amoroso, S., An, Y., Baxter, S., Bayatmakou, M., Becerril Gonzalez, H., Behnke, O., Belvedere, A., Bhattacharya, S., Blekman, F., Borras, K., Brunner, D., Campbell, A., Cardini, A., Cheng, C., Colombina, F., Consuegra Rodríguez, S., Correia Silva, G., De Silva, M., Eckerlin, G., Eckstein, D., Estevez Banos, L. I., Filatov, O., Gallo, E., Geiser, A., Giraldi, A., Greau, G., Guglielmi, V., Guthoff, M., Hinzmann, A., Jafari, A., Jeppe, L., Jomhari, N. Z., Kaech, B., Kasemann, M., Kaveh, H., Kleinwort, C., Kogler, R., Komm, M., Krücker, D., Lange, W., Leyva Pernia, D., Lipka, K., Lohmann, W., Mankel, R., Melzer-Pellmann, I.-A., Mendizabal Morentin, M., Metwally, J., Meyer, A. B., Milella, G., Mussgiller, A., Nürnberg, A., Otarid, Y., Pérez Adán, D., Ranken, E., Raspereza, A., Ribeiro Lopes, B., Rübenach, J., Saggio, A., Scham, M., Schnake, S., Schütze, P., Schwanenberger, C., Selivanova, D., Shchedrolosiev, M., Sosa Ricardo, R. E., Sreelatha Pramod, L. P., Stafford, D., Vazzoler, F., Ventura Barroso, A., Walsh, R., Wang, Q., Wen, Y., Wichmann, K., Wiens, L., Wissing, C., Wuchterl, S., Yang, Y., Zimermmane Castro Santos, A., Albrecht, A., Albrecht, S., Antonello, M., Bein, S., Benato, L., Bonanomi, M., Connor, P., Eich, M., El Morabit, K., Fischer, Y., Fröhlich, A., Garbers, C., Garutti, E., Grohsjean, A., Hajheidari, M., Haller, J., Jabusch, H. R., Kasieczka, G., Keicher, P., Klanner, R., Korcari, W., Kramer, T., Kutzner, V., Labe, F., Lange, J., Lobanov, A., Matthies, C., Mehta, A., Moureaux, L., Mrowietz, M., Nigamova, A., Nissan, Y., Paasch, A., Pena Rodriguez, K. J., Quadfasel, T., Raciti, B., Rieger, M., Savoiu, D., Schindler, J., Schleper, P., Schröder, M., Schwandt, J., Sommerhalder, M., Stadie, H., Steinbrück, G., Tews, A., Wolf, M., Brommer, S., Burkart, M., Butz, E., Chwalek, T., Dierlamm, A., Droll, A., Faltermann, N., Giffels, M., Gottmann, A., Hartmann, F., Hofsaess, R., Horzela, M., Husemann, U., Klute, M., Koppenhöfer, R., Link, M., Lintuluoto, A., Maier, S., Mitra, S., Mormile, M., Müller, Th., Neukum, M., Oh, M., Quast, G., Rabbertz, K., Regnery, B., Shadskiy, N., Shvetsov, I., Simonis, H. J., Trevisani, N., Ulrich, R., van der Linden, J., Von Cube, R. F., Wassmer, M., Wieland, S., Wittig, F., Wolf, R., Wunsch, S., Zuo, X., Anagnostou, G., Assiouras, P., Daskalakis, G., Kyriakis, A., Papadopoulos, A., Stakia, A., Kontaxakis, P., Melachroinos, G., Panagiotou, A., Papavergou, I., Paraskevas, I., Saoulidou, N., Theofilatos, K., Tziaferi, E., Vellidis, K., Zisopoulos, I., Bakas, G., Chatzistavrou, T., Karapostoli, G., Kousouris, K., Papakrivopoulos, I., Siamarkou, E., Tsipolitis, G., Zacharopoulou, A., Adamidis, K., Bestintzanos, I., Evangelou, I., Foudas, C., Gianneios, P., Kamtsikis, C., Katsoulis, P., Kokkas, P., Kosmoglou Kioseoglou, P. G., Manthos, N., Papadopoulos, I., Strologas, J., Bartók, M., Hajdu, C., Horvath, D., Sikler, F., Veszpremi, V., Csanád, M., Farkas, K., Gadallah, M. M. A., Kadlecsik, Á., Major, P., Mandal, K., Pásztor, G., Rádl, A. J., Veres, G. I., Raics, P., Ujvari, B., Zilizi, G., Bencze, G., Czellar, S., Karancsi, J., Molnar, J., Szillasi, Z., Csorgo, T., Nemes, F., Novak, T., Babbar, J., Bansal, S., Beri, S. B., Bhatnagar, V., Chaudhary, G., Chauhan, S., Dhingra, N., Gupta, R., Kaur, A., Kaur, A., Kaur, H., Kaur, M., Kumar, S., Meena, M., Sandeep, K., Sheokand, T., Singh, J. B., Singla, A., Ahmed, A., Bhardwaj, A., Chhetri, A., Choudhary, B. C., Kumar, A., Naimuddin, M., Ranjan, K., Saumya, S., Acharya, S., Baradia, S., Barman, S., Bhattacharya, S., Bhowmik, D., Dutta, S., Dutta, S., Gomber, B., Palit, P., Saha, G., Sahu, B., Sarkar, S., Ameen, M. M., Behera, P. K., Behera, S. C., Chatterjee, S., Jana, P., Kalbhor, P., Komaragiri, J. R., Kumar, D., Panwar, L., Pradhan, R., Pujahari, P. R., Saha, N. R., Sharma, A., Sikdar, A. K., Verma, S., Aziz, T., Das, I., Dugad, S., Kumar, M., Mohanty, G. B., Suryadevara, P., Bala, A., Banerjee, S., Chatterjee, R. M., Guchait, M., Jain, Sh., Karmakar, S., Kumar, S., Majumder, G., Mazumdar, K., Mukherjee, S., Parolia, S., Thachayath, A., Bahinipati, S., Das, A. K., Kar, C., Maity, D., Mal, P., Mishra, T., Muraleedharan Nair Bindhu, V. 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S., Zarubin, A., Zhizhin, I., and Zhokin, A.
Published: 2024
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35. Observation of the Λb0→J/ψΞ-K+ decay

Author: Hayrapetyan, A., Tumasyan, A., Adam, W., Andrejkovic, J. W., Bergauer, T., Chatterjee, S., Damanakis, K., Dragicevic, M., Valle, A. Escalante Del, Hussain, P. S., Jeitler, M., Krammer, N., Liko, D., Mikulec, I., Schieck, J., Schöfbeck, R., Schwarz, D., Sonawane, M., Templ, S., Waltenberger, W., Wulz, C.-E., Darwish, M. R., Janssen, T., Mechelen, P. Van, Bols, E. S., D’Hondt, J., Dansana, S., De Moor, A., Delcourt, M., El Faham, H., Lowette, S., Makarenko, I., Müller, D., Sahasransu, A. R., Tavernier, S., Tytgat, M., Van Putte, S., Vannerom, D., Clerbaux, B., De Lentdecker, G., Favart, L., Hohov, D., Jaramillo, J., Khalilzadeh, A., Lee, K., Mahdavikhorrami, M., Malara, A., Paredes, S., Pétré, L., Postiau, N., Thomas, L., Bemden, M. Vanden, Velde, C. Vander, Vanlaer, P., De Coen, M., Dobur, D., Hong, Y., Knolle, J., Lambrecht, L., Mestdach, G., Rendón, C., Samalan, A., Skovpen, K., Bossche, N. Van Den, Wezenbeek, L., Benecke, A., Bruno, G., Caputo, C., Delaere, C., Donertas, I. S., Giammanco, A., Jaffel, K., Jain, Sa., Lemaitre, V., Lidrych, J., Mastrapasqua, P., Mondal, K., Tran, T. T., Wertz, S., Alves, G. A., Coelho, E., Hensel, C., De Oliveira, T. Menezes, Moraes, A., Teles, P. Rebello, Soeiro, M., Júnior, W. L. Aldá, Pereira, M. Alves Gallo, Filho, M. Barroso Ferreira, Malbouisson, H. Brandao, Carvalho, W., Chinellato, J., Da Costa, E. M., Da Silveira, G. G., De Jesus Damiao, D., De Souza, S. Fonseca, Martins, J., Herrera, C. Mora, Amarilo, K. Mota, Mundim, L., Nogima, H., Santoro, A., Sznajder, A., Thiel, M., Pereira, A. Vilela, Bernardes, C. A., Calligaris, L., Tomei, T. R. Fernandez Perez, Gregores, E. M., Mercadante, P. G., Novaes, S. F., Orzari, B., Padula, Sandra S., Aleksandrov, A., Antchev, G., Hadjiiska, R., Iaydjiev, P., Misheva, M., Shopova, M., Sultanov, G., Dimitrov, A., Ivanov, T., Litov, L., Pavlov, B., Petkov, P., Petrov, A., Shumka, E., Keshri, S., Thakur, S., Cheng, T., Guo, Q., Javaid, T., Mittal, M., Yuan, L., Bauer, G., Hu, Z., Liu, J., Yi, K., Chen, G. M., Chen, H. S., Chen, M., Iemmi, F., Jiang, C. H., Kapoor, A., Liao, H., Liu, Z.-A., Monti, F., Shahzad, M. A., Sharma, R., Song, J. N., Tao, J., Wang, C., Wang, J., Wang, Z., Zhang, H., Agapitos, A., Ban, Y., Levin, A., Li, C., Li, Q., Mao, Y., Qian, S. J., Sun, X., Wang, D., Yang, H., Zhang, L., Zhou, C., You, Z., Lu, N., Gao, X., Leggat, D., Okawa, H., Zhang, Y., Lin, Z., Lu, C., Xiao, M., Avila, C., Trujillo, D. A. Barbosa, Cabrera, A., Florez, C., Fraga, J., Vega, J. A. Reyes, Guisao, J. Mejia, Ramirez, F., Rodriguez, M., Alvarez, J. D. 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El, Fay, J., Gascon, S., Gouzevitch, M., Greenberg, C., Grenier, G., Ille, B., Laktineh, I. B., Lethuillier, M., Mirabito, L., Perries, S., Purohit, A., Donckt, M. Vander, Verdier, P., Xiao, J., Adamov, G., Lomidze, I., Tsamalaidze, Z., Botta, V., Feld, L., Klein, K., Lipinski, M., Meuser, D., Pauls, A., Röwert, N., Teroerde, M., Diekmann, S., Dodonova, A., Eich, N., Eliseev, D., Engelke, F., Erdmann, M., Fackeldey, P., Fischer, B., Hebbeker, T., Hoepfner, K., Ivone, F., Jung, A., Lee, M. Y., Mastrolorenzo, L., Merschmeyer, M., Meyer, A., Mukherjee, S., Noll, D., Novak, A., Nowotny, F., Pozdnyakov, A., Rath, Y., Redjeb, W., Rehm, F., Reithler, H., Sarkisovi, V., Schmidt, A., Sharma, A., Stein, A., Da Silva De Araujo, F. Torres, Vigilante, L., Wiedenbeck, S., Zaleski, S., Dziwok, C., Flügge, G., Ahmad, W. Haj, Kress, T., Nowack, A., Pooth, O., Stahl, A., Ziemons, T., Zotz, A., Petersen, H. Aarup, Martin, M. 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Sreelatha, Stafford, D., Vazzoler, F., Barroso, A. Ventura, Walsh, R., Wang, Q., Wen, Y., Wichmann, K., Wiens, L., Wissing, C., Wuchterl, S., Yang, Y., Santos, A. Zimermmane Castro, Albrecht, A., Albrecht, S., Antonello, M., Bein, S., Benato, L., Bonanomi, M., Connor, P., Eich, M., El Morabit, K., Fischer, Y., Fröhlich, A., Garbers, C., Garutti, E., Grohsjean, A., Hajheidari, M., Haller, J., Jabusch, H. R., Kasieczka, G., Keicher, P., Klanner, R., Korcari, W., Kramer, T., Kutzner, V., Labe, F., Lange, J., Lobanov, A., Matthies, C., Mehta, A., Moureaux, L., Mrowietz, M., Nigamova, A., Nissan, Y., Paasch, A., Rodriguez, K. J. Pena, Quadfasel, T., Raciti, B., Rieger, M., Savoiu, D., Schindler, J., Schleper, P., Schröder, M., Schwandt, J., Sommerhalder, M., Stadie, H., Steinbrück, G., Tews, A., Wolf, M., Brommer, S., Burkart, M., Butz, E., Chwalek, T., Dierlamm, A., Droll, A., Faltermann, N., Giffels, M., Gottmann, A., Hartmann, F., Hofsaess, R., Horzela, M., Husemann, U., Klute, M., Koppenhöfer, R., Link, M., Lintuluoto, A., Maier, S., Mitra, S., Mormile, M., Müller, Th., Neukum, M., Oh, M., Quast, G., Rabbertz, K., Regnery, B., Shadskiy, N., Shvetsov, I., Simonis, H. J., Trevisani, N., Ulrich, R., van der Linden, J., Cube, R. F. 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S., Zarubin, A., Zhizhin, I., and Zhokin, A.
Published: 2024
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36. Search for Higgs boson pair production with one associated vector boson in proton-proton collisions at s = 13 TeV

Author: Hayrapetyan, A., Tumasyan, A., Adam, W., Andrejkovic, J. W., Bergauer, T., Chatterjee, S., Damanakis, K., Dragicevic, M., Escalante Del Valle, A., Hussain, P. S., Jeitler, M., Krammer, N., Liko, D., Mikulec, I., Schieck, J., Schöfbeck, R., Schwarz, D., Sonawane, M., Templ, S., Waltenberger, W., Wulz, C.-E., Darwish, M. R., Janssen, T., Van Mechelen, P., Bols, E. S., D’Hondt, J., Dansana, S., De Moor, A., Delcourt, M., El Faham, H., Lowette, S., Makarenko, I., Müller, D., Sahasransu, A. R., Tavernier, S., Tytgat, M., Van Putte, S., Vannerom, D., Clerbaux, B., De Lentdecker, G., Favart, L., Hohov, D., Jaramillo, J., Khalilzadeh, A., Lee, K., Mahdavikhorrami, M., Malara, A., Paredes, S., Pétré, L., Postiau, N., Thomas, L., Vanden Bemden, M., Vander Velde, C., Vanlaer, P., De Coen, M., Dobur, D., Hong, Y., Knolle, J., Lambrecht, L., Mestdach, G., Rendón, C., Samalan, A., Skovpen, K., Van Den Bossche, N., Wezenbeek, L., Benecke, A., Bruno, G., Caputo, C., Delaere, C., Donertas, I. S., Giammanco, A., Jaffel, K., Jain, Sa., Lemaitre, V., Lidrych, J., Mastrapasqua, P., Mondal, K., Tran, T. T., Wertz, S., Alves, G. A., Coelho, E., Hensel, C., Menezes De Oliveira, T., Moraes, A., Rebello Teles, P., Soeiro, M., Aldá Júnior, W. L., Alves Gallo Pereira, M., Barroso Ferreira Filho, M., Brandao Malbouisson, H., Carvalho, W., Chinellato, J., Da Costa, E. M., Da Silveira, G. G., De Jesus Damiao, D., Fonseca De Souza, S., Martins, J., Mora Herrera, C., Mota Amarilo, K., Mundim, L., Nogima, H., Santoro, A., Silva Do Amaral, S. M., Sznajder, A., Thiel, M., Vilela Pereira, A., Bernardes, C. A., Calligaris, L., Fernandez Perez Tomei, T. R., Gregores, E. M., Mercadante, P. G., Novaes, S. F., Orzari, B., Padula, Sandra S., Aleksandrov, A., Antchev, G., Hadjiiska, R., Iaydjiev, P., Misheva, M., Shopova, M., Sultanov, G., Dimitrov, A., Ivanov, T., Litov, L., Pavlov, B., Petkov, P., Petrov, A., Shumka, E., Keshri, S., Thakur, S., Cheng, T., Guo, Q., Javaid, T., Mittal, M., Yuan, L., Bauer, G., Hu, Z., Yi, K., Chen, G. M., Chen, H. S., Chen, M., Iemmi, F., Jiang, C. H., Kapoor, A., Liao, H., Liu, Z.-A., Monti, F., Shahzad, M. A., Sharma, R., Song, J. N., Tao, J., Wang, C., Wang, J., Wang, Z., Zhang, H., Agapitos, A., Ban, Y., Levin, A., Li, C., Li, Q., Lyu, X., Mao, Y., Qian, S. J., Sun, X., Wang, D., Yang, H., Zhang, L., Zhou, C., You, Z., Lu, N., Gao, X., Leggat, D., Okawa, H., Zhang, Y., Lin, Z., Lu, C., Xiao, M., Avila, C., Barbosa Trujillo, D. A., Cabrera, A., Florez, C., Fraga, J., Reyes Vega, J. A., Mejia Guisao, J., Ramirez, F., Rodriguez, M., Ruiz Alvarez, J. 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A., Van Hove, P., Beauceron, S., Blancon, B., Boudoul, G., Chanon, N., Choi, J., Contardo, D., Depasse, P., Dozen, C., El Mamouni, H., Fay, J., Gascon, S., Gouzevitch, M., Greenberg, C., Grenier, G., Ille, B., Laktineh, I. B., Lethuillier, M., Mirabito, L., Perries, S., Vander Donckt, M., Verdier, P., Xiao, J., Adamov, G., Lomidze, I., Tsamalaidze, Z., Botta, V., Feld, L., Klein, K., Lipinski, M., Meuser, D., Pauls, A., Röwert, N., Teroerde, M., Diekmann, S., Dodonova, A., Eich, N., Eliseev, D., Engelke, F., Erdmann, M., Fackeldey, P., Fischer, B., Hebbeker, T., Hoepfner, K., Ivone, F., Jung, A., Lee, M. y., Mastrolorenzo, L., Merschmeyer, M., Meyer, A., Mukherjee, S., Noll, D., Novak, A., Nowotny, F., Pozdnyakov, A., Rath, Y., Redjeb, W., Rehm, F., Reithler, H., Sarkisovi, V., Schmidt, A., Schuler, S. 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B., Milella, G., Mussgiller, A., Nürnberg, A., Otarid, Y., Pérez Adán, D., Ranken, E., Raspereza, A., Ribeiro Lopes, B., Rübenach, J., Saggio, A., Scham, M., Schnake, S., Schütze, P., Schwanenberger, C., Selivanova, D., Shchedrolosiev, M., Sosa Ricardo, R. E., Sreelatha Pramod, L. P., Stafford, D., Vazzoler, F., Ventura Barroso, A., Walsh, R., Wang, Q., Wen, Y., Wichmann, K., Wiens, L., Wissing, C., Wuchterl, S., Yang, Y., Zimermmane Castro Santos, A., Albrecht, A., Albrecht, S., Antonello, M., Bein, S., Benato, L., Bonanomi, M., Connor, P., Eich, M., El Morabit, K., Fischer, Y., Fröhlich, A., Garbers, C., Garutti, E., Grohsjean, A., Hajheidari, M., Haller, J., Jabusch, H. R., Kasieczka, G., Keicher, P., Klanner, R., Korcari, W., Kramer, T., Kutzner, V., Labe, F., Lange, J., Lobanov, A., Matthies, C., Mehta, A., Moureaux, L., Mrowietz, M., Nigamova, A., Nissan, Y., Paasch, A., Pena Rodriguez, K. J., Quadfasel, T., Raciti, B., Rieger, M., Savoiu, D., Schindler, J., Schleper, P., Schröder, M., Schwandt, J., Sommerhalder, M., Stadie, H., Steinbrück, G., Tews, A., Wolf, M., Brommer, S., Burkart, M., Butz, E., Chwalek, T., Dierlamm, A., Droll, A., Faltermann, N., Giffels, M., Gottmann, A., Hartmann, F., Hofsaess, R., Horzela, M., Husemann, U., Klute, M., Koppenhöfer, R., Link, M., Lintuluoto, A., Maier, S., Mitra, S., Mormile, M., Müller, Th., Neukum, M., Oh, M., Quast, G., Rabbertz, K., Regnery, B., Shadskiy, N., Shvetsov, I., Simonis, H. J., Trevisani, N., Ulrich, R., van der Linden, J., Von Cube, R. 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N., Canepa, A., Cerati, G. B., Cheung, H. W. K., Chlebana, F., Cummings, G., Dickinson, J., Dutta, I., Elvira, V. D., Feng, Y., Freeman, J., Gandrakota, A., Gecse, Z., Gray, L., Green, D., Grummer, A., Grünendahl, S., Guerrero, D., Gutsche, O., Harris, R. M., Heller, R., Herwig, T. C., Hirschauer, J., Horyn, L., Jayatilaka, B., Jindariani, S., Johnson, M., Joshi, U., Klijnsma, T., Klima, B., Kwok, K. H. M., Lammel, S., Lincoln, D., Lipton, R., Liu, T., Madrid, C., Maeshima, K., Mantilla, C., Mason, D., McBride, P., Merkel, P., Mrenna, S., Nahn, S., Ngadiuba, J., Noonan, D., Papadimitriou, V., Pastika, N., Pedro, K., Pena, C., Ravera, F., Reinsvold Hall, A., Ristori, L., Sexton-Kennedy, E., Smith, N., Soha, A., Spiegel, L., Stoynev, S., Strait, J., Taylor, L., Tkaczyk, S., Tran, N. V., Uplegger, L., Vaandering, E. W., Zoi, I., Aruta, C., Avery, P., Bourilkov, D., Cadamuro, L., Chang, P., Cherepanov, V., Field, R. D., Koenig, E., Kolosova, M., Konigsberg, J., Korytov, A., Lo, K. H., Matchev, K., Menendez, N., Mitselmakher, G., Muthirakalayil Madhu, A., Rawal, N., Rosenzweig, D., Rosenzweig, S., Shi, K., Wang, J., Adams, T., Al Kadhim, A., Askew, A., Bower, N., Habibullah, R., Hagopian, V., Hashmi, R., Kim, R. S., Kim, S., Kolberg, T., Martinez, G., Prosper, H., Prova, P. R., Viazlo, O., Wulansatiti, M., Yohay, R., Zhang, J., Alsufyani, B., Baarmand, M. M., Butalla, S., Elkafrawy, T., Hohlmann, M., Kumar Verma, R., Rahmani, M., Adams, M. R., Bennett, C., Cavanaugh, R., Dittmer, S., Escobar Franco, R., Evdokimov, O., Gerber, C. E., Hofman, D. J., Lee, J. h., Lemos, D. S., Merrit, A. H., Mills, C., Nanda, S., Oh, G., Ozek, B., Pilipovic, D., Roy, T., Rudrabhatla, S., Tonjes, M. B., Varelas, N., Wang, X., Ye, Z., Yoo, J., Alhusseini, M., Blend, D., Dilsiz, K., Emediato, L., Karaman, G., Köseyan, O. K., Merlo, J.-P., Mestvirishvili, A., Nachtman, J., Neogi, O., Ogul, H., Onel, Y., Penzo, A., Snyder, C., Tiras, E., Blumenfeld, B., Corcodilos, L., Davis, J., Gritsan, A. V., Kang, L., Kyriacou, S., Maksimovic, P., Roguljic, M., Roskes, J., Sekhar, S., Swartz, M., Vámi, T. Á., Abreu, A., Alcerro Alcerro, L. F., Anguiano, J., Baringer, P., Bean, A., Flowers, Z., Grove, D., King, J., Krintiras, G., Lazarovits, M., Le Mahieu, C., Lindsey, C., Marquez, J., Minafra, N., Murray, M., Nickel, M., Pitt, M., Popescu, S., Rogan, C., Royon, C., Salvatico, R., Sanders, S., Smith, C., Wang, Q., Wilson, G., Allmond, B., Ivanov, A., Kaadze, K., Kalogeropoulos, A., Kim, D., Maravin, Y., Nam, K., Natoli, J., Roy, D., Sorrentino, G., Rebassoo, F., Wright, D., Adams, E., Baden, A., Baron, O., Belloni, A., Bethani, A., Chen, Y. M., Eno, S. C., Hadley, N. J., Jabeen, S., Kellogg, R. G., Koeth, T., Kronheim, B., Lai, Y., Lascio, S., Mignerey, A. C., Nabili, S., Palmer, C., Papageorgakis, C., Paranjpe, M. M., Wang, L., Wong, K., Bendavid, J., Busza, W., Cali, I. A., Chen, Y., D’Alfonso, M., Eysermans, J., Freer, C., Gomez-Ceballos, G., Goncharov, M., Harris, P., Hoang, D., Kovalskyi, D., Krupa, J., Lavezzo, L., Lee, Y.-J., Long, K., Mironov, C., Paus, C., Rankin, D., Roland, C., Roland, G., Rothman, S., Shi, Z., Stephans, G. S. F., Wang, J., Wang, Z., Wyslouch, B., Yang, T. J., Crossman, B., Joshi, B. M., Kapsiak, C., Krohn, M., Mahon, D., Mans, J., Marzocchi, B., Pandey, S., Revering, M., Rusack, R., Saradhy, R., Schroeder, N., Strobbe, N., Wadud, M. A., Cremaldi, L. M., Bloom, K., Bryson, M., Claes, D. R., Fangmeier, C., Golf, F., Hossain, J., Joo, C., Kravchenko, I., Reed, I., Siado, J. E., Snow, G. R., Tabb, W., Vagnerini, A., Wightman, A., Yan, F., Yu, D., Zecchinelli, A. G., Agarwal, G., Bandyopadhyay, H., Hay, L., Iashvili, I., Kharchilava, A., McLean, C., Morris, M., Nguyen, D., Pekkanen, J., Rappoccio, S., Rejeb Sfar, H., Williams, A., Alverson, G., Barberis, E., Haddad, Y., Han, Y., Krishna, A., Li, J., Lu, M., Madigan, G., Morse, D. M., Nguyen, V., Orimoto, T., Parker, A., Skinnari, L., Tishelman-Charny, A., Wang, B., Wood, D., Bhattacharya, S., Bueghly, J., Chen, Z., Hahn, K. A., Liu, Y., Miao, Y., Monk, D. G., Schmitt, M. H., Taliercio, A., Velasco, M., Band, R., Bucci, R., Castells, S., Cremonesi, M., Das, A., Goldouzian, R., Hildreth, M., Ho, K. W., Hurtado Anampa, K., Jessop, C., Lannon, K., Lawrence, J., Loukas, N., Lutton, L., Mariano, J., Marinelli, N., Mcalister, I., McCauley, T., Mcgrady, C., Mohrman, K., Moore, C., Musienko, Y., Nelson, H., Osherson, M., Ruchti, R., Townsend, A., Wayne, M., Yockey, H., Zarucki, M., Zygala, L., Basnet, A., Bylsma, B., Carrigan, M., Durkin, L. S., Hill, C., Joyce, M., Lesauvage, A., Nunez Ornelas, M., Wei, K., Winer, B. L., Yates, B. R., Addesa, F. M., Bouchamaoui, H., Das, P., Dezoort, G., Elmer, P., Frankenthal, A., Greenberg, B., Haubrich, N., Higginbotham, S., Kopp, G., Kwan, S., Lange, D., Loeliger, A., Marlow, D., Ojalvo, I., Olsen, J., Stickland, D., Tully, C., Malik, S., Bakshi, A. S., Barnes, V. E., Chandra, S., Chawla, R., Das, S., Gu, A., Gutay, L., Jones, M., Jung, A. W., Kondratyev, D., Koshy, A. M., Liu, M., Negro, G., Neumeister, N., Paspalaki, G., Piperov, S., Purohit, A., Scheurer, V., Schulte, J. F., Stojanovic, M., Thieman, J., Virdi, A. K., Wang, F., Xie, W., Dolen, J., Parashar, N., Pathak, A., Acosta, D., Baty, A., Carnahan, T., Dildick, S., Ecklund, K. M., Fernández Manteca, P. J., Freed, S., Gardner, P., Geurts, F. J. M., Kumar, A., Li, W., Miguel Colin, O., Padley, B. P., Redjimi, R., Rotter, J., Yigitbasi, E., Zhang, Y., Bodek, A., de Barbaro, P., Demina, R., Dulemba, J. L., Fallon, C., Garcia-Bellido, A., Hindrichs, O., Khukhunaishvili, A., Parygin, P., Popova, E., Taus, R., Van Onsem, G. P., Goulianos, K., Chiarito, B., Chou, J. P., Gershtein, Y., Halkiadakis, E., Hart, A., Heindl, M., Jaroslawski, D., Karacheban, O., Laflotte, I., Lath, A., Montalvo, R., Nash, K., Routray, H., Salur, S., Schnetzer, S., Somalwar, S., Stone, R., Thayil, S. A., Thomas, S., Vora, J., Wang, H., Acharya, H., Ally, D., Delannoy, A. G., Fiorendi, S., Holmes, T., Karunarathna, N., Lee, L., Nibigira, E., Spanier, S., Aebi, D., Ahmad, M., Bouhali, O., Dalchenko, M., Eusebi, R., Gilmore, J., Huang, T., Kamon, T., Kim, H., Luo, S., Malhotra, S., Mueller, R., Overton, D., Rathjens, D., Safonov, A., Akchurin, N., Damgov, J., Hegde, V., Hussain, A., Kazhykarim, Y., Lamichhane, K., Lee, S. W., Mankel, A., Mengke, T., Muthumuni, S., Peltola, T., Volobouev, I., Whitbeck, A., Appelt, E., Greene, S., Gurrola, A., Johns, W., Kunnawalkam Elayavalli, R., Melo, A., Romeo, F., Sheldon, P., Tuo, S., Velkovska, J., Viinikainen, J., Cardwell, B., Cox, B., Hakala, J., Hirosky, R., Ledovskoy, A., Li, A., Neu, C., Perez Lara, C. E., Karchin, P. E., Aravind, A., Banerjee, S., Black, K., Bose, T., Dasu, S., De Bruyn, I., Everaerts, P., Galloni, C., He, H., Herndon, M., Herve, A., Koraka, C. K., Lanaro, A., Loveless, R., Madhusudanan Sreekala, J., Mallampalli, A., Mohammadi, A., Mondal, S., Parida, G., Pinna, D., Savin, A., Shang, V., Sharma, V., Smith, W. H., Teague, D., Tsoi, H. F., Vetens, W., Warden, A., Afanasiev, S., Andreev, V., Andreev, Yu., Aushev, T., Azarkin, M., Babaev, A., Belyaev, A., Blinov, V., Boos, E., Borshch, V., Budkouski, D., Bunichev, V., Chekhovsky, V., Chistov, R., Danilov, M., Dermenev, A., Dimova, T., Druzhkin, D., Dubinin, M., Dudko, L., Ershov, A., Gavrilov, G., Gavrilov, V., Gninenko, S., Golovtcov, V., Golubev, N., Golutvin, I., Gorbunov, I., Gribushin, A., Ivanov, Y., Kachanov, V., Kardapoltsev, L., Karjavine, V., Karneyeu, A., Kim, V., Kirakosyan, M., Kirpichnikov, D., Kirsanov, M., Klyukhin, V., Kodolova, O., Konstantinov, D., Korenkov, V., Kozyrev, A., Krasnikov, N., Lanev, A., Levchenko, P., Lychkovskaya, N., Makarenko, V., Malakhov, A., Matveev, V., Murzin, V., Nikitenko, A., Obraztsov, S., Oreshkin, V., Palichik, V., Perelygin, V., Perfilov, M., Petrushanko, S., Polikarpov, S., Popov, V., Radchenko, O., Savina, M., Savrin, V., Shalaev, V., Shmatov, S., Shulha, S., Skovpen, Y., Slabospitskii, S., Smirnov, V., Sosnov, D., Sulimov, V., Tcherniaev, E., Terkulov, A., Teryaev, O., Tlisova, I., Toropin, A., Uvarov, L., Uzunian, A., Vorobyev, A., Voytishin, N., Yuldashev, B. S., Zarubin, A., Zhizhin, I., and Zhokin, A.
Published: 2024
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37. Ground-state mass of $^{22}$Al and test of state-of-the-art \textit{ab initio} calculations

Author: Sun, M. Z., Yu, Y., Wang, X. P., Wang, M., Li, J. G., Zhang, Y. H., Blaum, K., Chen, Z. Y., Chen, R. J., Deng, H. Y., Fu, C. Y., Ge, W. W., Huang, W. J., Jiao, H. Y., Li, H. H., Li, H. F., Luo, Y. F., Liao, T., Litvinov, Yu. A., Si, M., Shuai, P., Shi, J. Y., Wang, Q., Xing, Y. M., Xu, X., Xu, H. S., Xu, F. R., Yuan, Q., Yamaguchi, T., Yan, X. L., Yang, J. C., Yuan, Y. J., Zhou, X. H., Zhou, X., Zhang, M., and Zeng, Q.
Subjects: Nuclear Experiment
Abstract: The ground-state mass excess of the $T_{z}=-2$ drip-line nucleus $^{22}$Al is measured for the first time to be $18103(10)$ keV using the newly-developed B$\rho$-defined isochronous mass spectrometry method at the cooler storage ring in Lanzhou. The new mass excess value allowed us to determine the excitation energies of the two low-lying $1^+$ states in $^{22}$Al with significantly reduced uncertainties of 51 keV. Comparing to the analogue states in its mirror nucleus $^{22}$F, the mirror energy differences of the two $1^+$ states in the $^{22}$Al-$^{22}$F mirror pair are determined to be $-625(51)$ keV and $-330(51)$ keV, respectively. The excitation energies and the mirror energy differences are used to test the state-of-the-art \textit{ab initio} valence-space in-medium similarity renormalization group calculations with four sets of interactions derived from the chiral effective field theory. The mechanism leading to the large mirror energy differences is investigated and attributed to the occupation of the $\pi s_{1/2}$ orbital., Comment: 8 pages, 5 figures
Published: 2024

38. X-ray detection of the most extreme star-forming galaxies at the cosmic noon via strong lensing

Author: Wang, Q. Daniel, Diaz, Carlos Garcia, Kamieneski, Patrick S., Harrington, Kevin C., Yun, Min S., Foo, Nicholas, Frye, Brenda L., Jimenez-Andrade, Eric F., Liu, Daizhong, Lowenthal, James D., Pampliega, Belen Alcalde, Pascale, Massimo, Vishwas, Amit, and Gurwell, Mark A.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract: Hyper-luminous infrared galaxies (HyLIRGs) are the most extreme star-forming systems observed in the early Universe, and their properties still elude comprehensive understanding. We have undertaken a large XMM-Newton observing program to probe the total accreting black hole population in three HyLIRGs at z = 2.12, 3.25, and 3.55, gravitationally lensed by foreground galaxies. Selected from the Planck All-Sky Survey to Analyze Gravitationally-lensed Extreme Starbursts (PASSAGES), these HyLIRGs have apparent infrared luminosities > E14 Lsun. Our observations revealed X-ray emission in each of them. PJ1336+49 appears to be dominated by high-mass X-ray binaries (HMXBs). Remarkably, the luminosity of this non-AGN X-ray emission exceeds by a factor of about three the value obtained by calibration with local galaxies with much lower star formation rates. This enhanced X-ray emission most likely highlights the efficacy of dynamical HMXB production within compact clusters, which is an important mode of star formation in HyLIRGs. The remaining two (PJ0116-24 and PJ1053+60) morphologically and spectrally exhibit a compact X-ray component in addition to the extended non-AGN X-ray emission, indicating the presence of Active Galactic Nuclei (AGNs). The AGN appears to be centrally located in the reconstructed source plane images of PJ0116-24, which manifests its star-forming activity predominantly within an extended galactic disk. In contrast, the AGN in the field of PJ1053+60 is projected 60 kpc away from the extreme star-forming galaxy and could be ejected from it. These results underline the synergistic potential of deep X-ray observations with strong lensing for the study of high-energy astrophysical phenomena in HyLIRGs., Comment: Just accepted for publication in MNRAS; comments are welcome
Published: 2023

39. Observation of the distribution of nuclear magnetization in a molecule

Author: Wilkins, S. G., Udrescu, S. M., Athanasakis-Kaklamanakis, M., Ruiz, R. F. Garcia, Au, M., Belošević, I., Berger, R., Bissell, M. L., Breier, A. A., Brinson, A. J., Chrysalidis, K., Cocolios, T. E., de Groote, R. P., Dorne, A., Flanagan, K. T., Franchoo, S., Gaul, K., Geldhof, S., Giesen, T. F., Hanstorp, D., Heinke, R., Isaev, T., Koszorús, Á., Kujanpää, S., Lalanne, L., Neyens, G., Nichols, M., Perrett, H. A., Reilly, J. R., Skripnikov, L. V., Rothe, S., Borne, B. van den, Wang, Q., Wessolek, J., Yang, X. F., and Zülch, C.
Subjects: Nuclear Experiment, Physics - Atomic Physics, Physics - Chemical Physics, Physics - Computational Physics
Abstract: Rapid progress in the experimental control and interrogation of molecules, combined with developments in precise calculations of their structure, are enabling new opportunities in the investigation of nuclear and particle physics phenomena. Molecules containing heavy, octupole-deformed nuclei such as radium are of particular interest for such studies, offering an enhanced sensitivity to the properties of fundamental particles and interactions. Here, we report precision laser spectroscopy measurements and theoretical calculations of the structure of the radioactive radium monofluoride molecule, $^{225}$Ra$^{19}$F. Our results allow fine details of the short-range electron-nucleus interaction to be revealed, indicating the high sensitivity of this molecule to the distribution of magnetization, currently a poorly constrained nuclear property, within the radium nucleus. These results provide a direct and stringent test of the description of the electronic wavefunction inside the nuclear volume, highlighting the suitability of these molecules to investigate subatomic phenomena.
Published: 2023

40. Nanoscale electronic inhomogeneities in 1T-TaS$_2$

Author: Campbell, B., Riffle, J. V., de la Torre, A., Wang, Q., Plumb, K. W., and Hollen, S. M.
Subjects: Condensed Matter - Mesoscale and Nanoscale Physics, Condensed Matter - Strongly Correlated Electrons
Abstract: We report a set of scanning tunneling microscopy (STM) and spectroscopy (STS) experiments studying native defects in CVT grown 1T-TaS$_2$. Six different sample surfaces from four bulk crystals were investigated. Wide area imaging reveals a prevalence of nanometer-scale electronic inhomogeneities due to native defects, with pristine regions interspersed. These inhomogeneities appear in typical as-grown crystals and coexist with a well-formed commensurate charge density wave of 1T-TaS$_2$ at low temperatures. Electronic inhomogeneities show up both as variations in the apparent height in STM and in the local density of states in STS; the bands can shift by 60 meV and the gap varies by more than 100 meV across inhomogeneities. These inhomogeneities are present in similar concentration across large-scale areas of all samples studied, but do not influence the charge density wave formation on local or global scales. The commensurate charge density wave exhibits long-range order and remains locally intact in the presence of these inhomogeneities., Comment: 5 pages, 5 figures
Published: 2023

41. LEM All-Sky Survey: Soft X-ray Sky at Microcalorimeter Resolution

Author: Khabibullin, Ildar, Galeazzi, Massimiliano, Bogdan, Akos, Cann, Jenna M., Churazov, Eugene, Dolag, Klaus, Drake, Jeremy J., Forman, William, Hernquist, Lars, Koutroumpa, Dimitra, Kraft, Ralph, Kuntz, K. D., Markevitch, Maxim, McCammon, Dan, Ogorzalek, Anna, Pfeifle, Ryan, Pillepich, Annalisa, Plucinsky, Paul P., Ponti, Gabriele, Schellenberger, Gerrit, Truong, Nhut, Valentini, Milena, Veilleux, Sylvain, Vladutescu-Zopp, Stephan, Wang, Q. Daniel, and Weaver, Kimberly
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Solar and Stellar Astrophysics
Abstract: The Line Emission Mapper (LEM) is an X-ray Probe with with spectral resolution ~2 eV FWHM from 0.2 to 2.5 keV and effective area >2,500 cm$^2$ at 1 keV, covering a 33 arcmin diameter Field of View with 15 arcsec angular resolution, capable of performing efficient scanning observations of very large sky areas and enabling the first high spectral resolution survey of the full sky. The LEM-All-Sky Survey (LASS) is expected to follow the success of previous all sky surveys such as ROSAT and eROSITA, adding a third dimension provided by the high resolution microcalorimeter spectrometer, with each 15 arcsec pixel of the survey including a full 1-2 eV resolution energy spectrum that can be integrated over any area of the sky to provide statistical accuracy. Like its predecessors, LASS will provide both a long-lasting legacy and open the door to the unknown, enabling new discoveries and delivering the baseline for unique GO studies. No other current or planned mission has the combination of microcalorimeter energy resolution and large grasp to cover the whole sky while maintaining good angular resolution and imaging capabilities. LASS will be able to probe the physical conditions of the hot phases of the Milky Way at multiple scales, from emission in the Solar system due to Solar Wind Charge eXchange, to the interstellar and circumgalactic media, including the North Polar Spur and the Fermi/eROSITA bubbles. It will measure velocities of gas in the inner part of the Galaxy and extract the emissivity of the Local Hot Bubble. By maintaining the original angular resolution, LASS will also be able to study classes of point sources through stacking. For classes with ~$10^4$ objects, it will provide the equivalent of 1 Ms of high spectral resolution data. We describe the technical specifications of LASS and highlight the main scientific objectives that will be addressed. (Abridged), Comment: White Paper in support of a mission concept to be submitted for the 2023 NASA Astrophysics Probes opportunity. This White Paper will be updated when required. 30 pages, 25 figures
Published: 2023

42. Experimental Limits on Solar Reflected Dark Matter with a New Approach on Accelerated-Dark-Matter-Electron Analysis in Semiconductors

Author: Zhang, Z. Y., Yang, L. T., Yue, Q., Kang, K. J., Li, Y. J., An, H. P., C., Greeshma, Chang, J. P., Chen, Y. H., Cheng, J. P., Dai, W. H., Deng, Z., Fang, C. H., Geng, X. P., Gong, H., Guo, Q. J., Guo, T., Guo, X. Y., He, L., He, S. M., Hu, J. W., Huang, H. X., Huang, T. C., Jiang, L., Karmakar, S., Li, H. B., Li, H. Y., Li, J. M., Li, J., Li, Q. Y., Li, R. M. J., Li, X. Q., Li, Y. L., Liang, Y. F., Liao, B., Lin, F. K., Lin, S. T., Liu, J. X., Liu, S. K., Liu, Y. D., Liu, Y., Liu, Y. Y., Ma, H., Mao, Y. C., Nie, Q. Y., Ning, J. H., Pan, H., Qi, N. C., Ren, J., Ruan, X. C., Singh, M. K., Sun, T. X., Tang, C. J., Tian, Y., Wang, G. F., Wang, J. Z., Wang, L., Wang, Q., Wang, Y. F., Wang, Y. X., Wong, H. T., Wu, S. Y., Wu, Y. C., Xing, H. Y., Xu, R., Xu, Y., Xue, T., Yan, Y. L., Yi, N., Yu, C. X., Yu, H. J., Yue, J. F., Zeng, M., Zeng, Z., Zhang, B. T., Zhang, F. S., Zhang, L., Zhang, Z. H., Zhao, J. Z., Zhao, K. K., Zhao, M. G., Zhou, J. F., Zhou, Z. Y., and Zhu, J. J.
Subjects: High Energy Physics - Experiment, High Energy Physics - Phenomenology, Physics - Instrumentation and Detectors
Abstract: Recently a dark matter-electron (DM-electron) paradigm has drawn much attention. Models beyond the standard halo model describing DM accelerated by high energy celestial bodies are under intense examination as well. In this Letter, a velocity components analysis (VCA) method dedicated to swift analysis of accelerated DM-electron interactions via semiconductor detectors is proposed and the first HPGe detector-based accelerated DM-electron analysis is realized. Utilizing the method, the first germanium based constraint on sub-GeV solar reflected DM-electron interaction is presented with the 205.4 kg$\cdot$day dataset from the CDEX-10 experiment. In the heavy mediator scenario, our result excels in the mass range of 5$-$15 keV/$c^2$, achieving a 3 orders of magnitude improvement comparing with previous semiconductor experiments. In the light mediator scenario, the strongest laboratory constraint for DM lighter than 0.1 MeV/$c^2$ is presented. The result proves the feasibility and demonstrates the vast potential of the VCA technique in future accelerated DM-electron analyses with semiconductor detectors., Comment: 7 pages, 4 figures. Version updated to match PRL version
Published: 2023
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43. X-rays Trace the Volatile Content of Interstellar Objects

Author: Cabot, Samuel H. C., Wang, Q. Daniel, and Seligman, Darryl Z.
Subjects: Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract: The non-detection of a coma surrounding 1I/`Oumuamua, the first discovered interstellar object (ISO), has prompted a variety of hypotheses to explain its nongravitational acceleration. Given that forthcoming surveys are poised to identify analogues of this enigmatic object, it is prudent to devise alternative approaches to characterization. In this study, we posit X-ray spectroscopy as a surprisingly effective probe of volatile ISO compositions. Heavily ionized metals in the solar wind interact with outgassed neutrals and emit high-energy photons in a process known as charge exchange, and charge exchange induced X-rays from comets and planetary bodies have been observed extensively in our Solar System. We develop a model to predict the X-ray flux of an ISO based on its chemical inventory and ephemeris. We find that while standard cometary constituents, such as H$_2$O, CO$_2$, CO, and dust are best probed via optical or infrared observations, we predict strong X-ray emission generated by charge exchange with extended comae of H$_2$ and N$_2$ -- species which lack strong infrared fluorescence transitions. We find that XMM-Newton would have been sensitive to charge exchange emission from 1I/`Oumuamua during the object's close approach to Earth, and that constraints on composition may have been feasible. We argue for follow-up X-ray observations of newly discovered ISOs with close-in perihelia. Compositional constraints on the general ISO population could reconcile the apparently self-conflicting nature of 1I/`Oumuamua, and provide insight into the earliest stages of planet formation in extrasolar systems., Comment: Accepted to The Astrophysical Journal. 18 pages, 6 figures
Published: 2023

44. Keck Infrared Transient Survey I: Survey Description and Data Release 1

Author: Tinyanont, S., Foley, R. J., Taggart, K., Davis, K. W., LeBaron, N., Andrews, J. E., Bustamante-Rosell, M. J., Camacho-Neves, Y., Chornock, R., Coulter, D. A., Galbany, L., Jha, S. W., Kilpatrick, C. D., Kwok, L. A., Larison, C., Pierel, J. R., Siebert, M. R., Aldering, G., Auchettl, K., Bloom, J. S., Dhawan, S., Filippenko, A. V., French, K. D., Gagliano, A., Grayling, M., Jacobson-Galán, W. V., Jones, D. O., Saux, X. Le, Macias, P., Mandel, K. S., McCully, C., Gonzalez, E. Padilla, Rest, A., Rojas-Bravo, C., Skrutskie, M. F., Thorp, S., Wang, Q., and Ward, S. M.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: We present the Keck Infrared Transient Survey (KITS), a NASA Key Strategic Mission Support program to obtain near-infrared (NIR) spectra of astrophysical transients of all types, and its first data release, consisting of 105 NIR spectra of 50 transients. Such a data set is essential as we enter a new era of IR astronomy with the James Webb Space Telescope (JWST) and the upcoming Nancy Grace Roman Space Telescope (Roman). NIR spectral templates will be essential to search JWST images for stellar explosions of the first stars and to plan an effective Roma} SN Ia cosmology survey, both key science objectives for mission success. Between 2022 February and 2023 July, we systematically obtained 274 NIR spectra of 146 astronomical transients, representing a significant increase in the number of available NIR spectra in the literature. The first data release includes data from the 2022A semester. We systematically observed three samples: a flux-limited sample that includes all transients $<$17 mag in a red optical band (usually ZTF r or ATLAS o bands); a volume-limited sample including all transients within redshift $z < 0.01$ ($D \approx 50$ Mpc); and an SN Ia sample targeting objects at phases and light-curve parameters that had scant existing NIR data in the literature. The flux-limited sample is 39% complete (60% excluding SNe Ia), while the volume-limited sample is 54% complete and is 79% complete to $z = 0.005$. All completeness numbers will rise with the inclusion of data from other telescopes in future data releases. Transient classes observed include common Type Ia and core-collapse supernovae, tidal disruption events (TDEs), luminous red novae, and the newly categorized hydrogen-free/helium-poor interacting Type Icn supernovae. We describe our observing procedures and data reduction using Pypeit, which requires minimal human interaction to ensure reproducibility.
Published: 2023

45. Tracing the Energetic Outflows from Galactic Nuclei: Observational Evidence for a Large-Scale Bipolar Radio and X-ray-emitting Bubble-like Structure in M106

Author: Zeng, Yuxuan, Wang, Q. Daniel, and Fraternali, Filippo
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Astrophysics of Galaxies, Physics - Plasma Physics
Abstract: The role of energetic outflows from galactic nuclei in shaping galaxy formation and evolution is still shrouded in uncertainty. In this study, we shed light on this complex phenomenon by presenting evidence for a large-scale bipolar radio/X-ray-emitting bubble-like structure emanating from the central region of the nearby disk galaxy M106 (NGC 4258). Our findings, based on Low-Frequency Array survey data and Chandra observations, provide a glimpse into the underlying physical processes driving this enigmatic structure. Similar to the eROSITA/Fermi bubbles in our own Galaxy, the M106 bubbles enclose diffuse hot plasma and are partially bounded by prominent radio/X-ray-emitting edges. We constrain the magnetic field and cosmic-ray properties of the structure. The analysis of the X-ray data gives an estimate of the thermal energy of the bubbles as ~8 x 10^56 erg. This energy can be supplied by the jets and perhaps by the wind from the accretion flow of the galaxy's low-luminosity AGN, which most likely has been much more powerful in the recent past, with an average mechanical energy release rate of ~4 x 10^42 erg/s over the last ~ 8 x 10^6 yr -- the estimated age of the structure. We also show evidence for diffuse X-ray emission on larger scales, indicating the presence of a hot galactic corona. Our results provide a clear manifestation of galactic nuclear feedback regulating the gas content and energetics of the circumgalactic medium of disk galaxies similar to our own., Comment: Just accepted for publication in MNRAS; comments are welcome
Published: 2023

46. Projected WIMP sensitivity of the CDEX-50 dark matter experiment

Author: Geng, X. P., Yang, L. T., Yue, Q., Kang, K. J., Li, Y. J., An, H. P., C., Greeshma, Chang, J. P., Chen, Y. H., Cheng, J. P., Dai, W. H., Deng, Z., Fang, C. H., Gong, H., Guo, Q. J., Guo, T., Guo, X. Y., He, L., He, S. M., Hu, J. W., Huang, H. X., Huang, T. C., Jiang, L., Karmakar, S., Li, H. B., Li, H. Y., Li, J. M., Li, J., Li, Q. Y., Li, R. M. J., Li, X. Q., Li, Y. L., Liang, Y. F., Liao, B., Lin, F. K., Lin, S. T., Liu, J. X., Liu, S. K., Liu, Y. D., Liu, Y., Liu, Y. Y., Ma, H., Mao, Y. C., Nie, Q. Y., Ning, J. H., Pan, H., Qi, N. C., Ren, J., Ruan, X. C., Singh, M. K., Sun, T. X., Tang, C. J., Tian, Y., Wang, G. F., Wang, J. Z., Wang, L., Wang, Q., Wang, Y. F., Wang, Y. X., Wong, H. T., Wu, S. Y., Wu, Y. C., Xing, H. Y., Xu, R., Xu, Y., Xue, T., Yan, Y. L., Yi, N., Yu, C. X., Yu, H. J., Yue, J. F., Zeng, M., Zeng, Z., Zhang, B. T., Zhang, F. S., Zhang, L., Zhang, Z. H., Zhang, Z. Y., Zhao, J. Z., Zhao, K. K., Zhao, M. G., Zhou, J. F., Zhou, Z. Y., and Zhu, J. J.
Subjects: High Energy Physics - Experiment, Physics - Instrumentation and Detectors
Abstract: CDEX-50 is a next-generation project of the China Dark Matter Experiment (CDEX) that aims to search for dark matter using a 50-kg germanium detector array. This paper comprises a thorough summary of the CDEX-50 dark matter experiment, including an investigation of potential background sources and the development of a background model. Based on the baseline model, the projected sensitivity of weakly interacting massive particle (WIMP) is also presented. The expected background level within the energy region of interest, set to 2--2.5 keVee, is $\sim$0.01 counts keVee$^{-1}$ kg$^{-1}$ day$^{-1}$. At 90\% confidence level, the expected sensitivity to spin-independent WIMP-nucleon couplings is estimated to reach a cross-section of 5.1 $\times$ 10$^{-45}$ cm$^{2}$ for a WIMP mass of 5 GeV/c$^{2}$ with an exposure objective of 150 kg$\cdot$year and an analysis threshold of 160 eVee. This science goal will correspond to the most sensitive results for WIMPs with a mass of 2.2--8 GeV/c$^{2}$., Comment: 12 pages, 11 figures. Version updated to match JCAP version
Published: 2023
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47. Comparing recent PTA results on the nanohertz stochastic gravitational wave background

Author: The International Pulsar Timing Array Collaboration, Agazie, G., Antoniadis, J., Anumarlapudi, A., Archibald, A. M., Arumugam, P., Arumugam, S., Arzoumanian, Z., Askew, J., Babak, S., Bagchi, M., Bailes, M., Nielsen, A. -S. Bak, Baker, P. T., Bassa, C. G., Bathula, A., Bécsy, B., Berthereau, A., Bhat, N. D. R., Blecha, L., Bonetti, M., Bortolas, E., Brazier, A., Brook, P. R., Burgay, M., Burke-Spolaor, S., Burnette, R., Caballero, R. N., Cameron, A., Case, R., Chalumeau, A., Champion, D. J., Chanlaridis, S., Charisi, M., Chatterjee, S., Chatziioannou, K., Cheeseboro, B. D., Chen, S., Chen, Z. -C., Cognard, I., Cohen, T., Coles, W. A., Cordes, J. M., Cornish, N. J., Crawford, F., Cromartie, H. T., Crowter, K., Curyło, M., Cutler, C. J., Dai, S., Dandapat, S., Deb, D., DeCesar, M. E., DeGan, D., Demorest, P. B., Deng, H., Desai, S., Desvignes, G., Dey, L., Dhanda-Batra, N., Di Marco, V., Dolch, T., Drachler, B., Dwivedi, C., Ellis, J. A., Falxa, M., Feng, Y., Ferdman, R. D., Ferrara, E. C., Fiore, W., Fonseca, E., Franchini, A., Freedman, G. E., Gair, J. R., Garver-Daniels, N., Gentile, P. A., Gersbach, K. A., Glaser, J., Good, D. C., Goncharov, B., Gopakumar, A., Graikou, E., Grießmeier, J. -M., Guillemot, L., Gültekin, K., Guo, Y. J., Gupta, Y., Grunthal, K., Hazboun, J. S., Hisano, S., Hobbs, G. B., Hourihane, S., Hu, H., Iraci, F., Islo, K., Izquierdo-Villalba, D., Jang, J., Jawor, J., Janssen, G. H., Jennings, R. J., Jessner, A., Johnson, A. D., Jones, M. L., Joshi, B. C., Kaiser, A. R., Kaplan, D. L., Kapur, A., Kareem, F., Karuppusamy, R., Keane, E. F., Keith, M. J., Kelley, L. Z., Kerr, M., Key, J. S., Kharbanda, D., Kikunaga, T., Klein, T. C., Kolhe, N., Kramer, M., Krishnakumar, M. A., Kulkarni, A., Laal, N., Lackeos, K., Lam, M. T., Lamb, W. G., Larsen, B. B., Lazio, T. J. W., Lee, K. J., Levin, Y., Lewandowska, N., Littenberg, T. B., Liu, K., Liu, T., Liu, Y., Lommen, A., Lorimer, D. R., Lower, M. E., Luo, J., Luo, R., Lynch, R. S., Lyne, A. G., Ma, C. -P., Maan, Y., Madison, D. R., Main, R. A., Manchester, R. N., Mandow, R., Mattson, M. A., McEwen, A., McKee, J. W., McLaughlin, M. A., McMann, N., Meyers, B. W., Meyers, P. M., Mickaliger, M. B., Miles, M., Mingarelli, C. M. F., Mitridate, A., Natarajan, P., Nathan, R. S., Ng, C., Nice, D. J., Niţu, I. C., Nobleson, K., Ocker, S. K., Olum, K. D., Osłowski, S., Paladi, A. K., Parthasarathy, A., Pennucci, T. T., Perera, B. B. P., Perrodin, D., Petiteau, A., Petrov, P., Pol, N. S., Porayko, N. K., Possenti, A., Prabu, T., Leclere, H. Quelquejay, Radovan, H. A., Rana, P., Ransom, S. M., Ray, P. S., Reardon, D. J., Rogers, A. F., Romano, J. D., Russell, C. J., Samajdar, A., Sanidas, S. A., Sardesai, S. C., Schmiedekamp, A., Schmiedekamp, C., Schmitz, K., Schult, L., Sesana, A., Shaifullah, G., Shannon, R. M., Shapiro-Albert, B. J., Siemens, X., Simon, J., Singha, J., Siwek, M. S., Speri, L., Spiewak, R., Srivastava, A., Stairs, I. H., Stappers, B. W., Stinebring, D. R., Stovall, K., Sun, J. P., Surnis, M., Susarla, S. C., Susobhanan, A., Swiggum, J. K., Takahashi, K., Tarafdar, P., Taylor, J., Taylor, S. R., Theureau, G., Thrane, E., Thyagarajan, N., Tiburzi, C., Toomey, L., Turner, J. E., Unal, C., Vallisneri, M., van der Wateren, E., van Haasteren, R., Vecchio, A., Krishnan, V. Venkatraman, Verbiest, J. P. W., Vigeland, S. J., Wahl, H. M., Wang, S., Wang, Q., Witt, C. A., Wang, J., Wang, L., Wayt, K. E., Wu, Z., Young, O., Zhang, L., Zhang, S., Zhu, X. -J., and Zic, A.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, General Relativity and Quantum Cosmology
Abstract: The Australian, Chinese, European, Indian, and North American pulsar timing array (PTA) collaborations recently reported, at varying levels, evidence for the presence of a nanohertz gravitational wave background (GWB). Given that each PTA made different choices in modeling their data, we perform a comparison of the GWB and individual pulsar noise parameters across the results reported from the PTAs that constitute the International Pulsar Timing Array (IPTA). We show that despite making different modeling choices, there is no significant difference in the GWB parameters that are measured by the different PTAs, agreeing within $1\sigma$. The pulsar noise parameters are also consistent between different PTAs for the majority of the pulsars included in these analyses. We bridge the differences in modeling choices by adopting a standardized noise model for all pulsars and PTAs, finding that under this model there is a reduction in the tension in the pulsar noise parameters. As part of this reanalysis, we "extended" each PTA's data set by adding extra pulsars that were not timed by that PTA. Under these extensions, we find better constraints on the GWB amplitude and a higher signal-to-noise ratio for the Hellings and Downs correlations. These extensions serve as a prelude to the benefits offered by a full combination of data across all pulsars in the IPTA, i.e., the IPTA's Data Release 3, which will involve not just adding in additional pulsars, but also including data from all three PTAs where any given pulsar is timed by more than as single PTA., Comment: 21 pages, 9 figures, submitted to ApJ
Published: 2023

48. Measurement of the Bs0→J/ψKS0s effective lifetime from proton-proton collisions at Bs0→J/ψKS0s = 13 TeV

Author: Hayrapetyan, A., Tumasyan, A., Adam, W., Andrejkovic, J. W., Bergauer, T., Chatterjee, S., Damanakis, K., Dragicevic, M., Hussain, P. S., Jeitler, M., Krammer, N., Li, A., Liko, D., Mikulec, I., Schieck, J., Schöfbeck, R., Schwarz, D., Sonawane, M., Waltenberger, W., Wulz, C.-E., Janssen, T., Van Laer, T., Van Mechelen, P., Breugelmans, N., D’Hondt, J., Dansana, S., De Moor, A., Delcourt, M., Heyen, F., Lowette, S., Makarenko, I., Müller, D., Tavernier, S., Tytgat, M., Van Onsem, G. P., Van Putte, S., Vannerom, D., Bilin, B., Clerbaux, B., Das, A. K., De Lentdecker, G., Evard, H., Favart, L., Gianneios, P., Jaramillo, J., Khalilzadeh, A., Khan, F. A., Lee, K., Mahdavikhorrami, M., Malara, A., Paredes, S., Shahzad, M. A., Thomas, L., Vanden Bemden, M., Vander Velde, C., Vanlaer, P., De Coen, M., Dobur, D., Gokbulut, G., Hong, Y., Knolle, J., Lambrecht, L., Marckx, D., Mota Amarilo, K., Samalan, A., Skovpen, K., Van Den Bossche, N., van der Linden, J., Wezenbeek, L., Benecke, A., Bethani, A., Bruno, G., Caputo, C., De Favereau De Jeneret, J., Delaere, C., Donertas, I. S., Giammanco, A., Guzel, A. O., Jain, Sa., Lemaitre, V., Lidrych, J., Mastrapasqua, P., Tran, T. T., Wertz, S., Alves, G. A., Alves Gallo Pereira, M., Coelho, E., Correia Silva, G., Hensel, C., Menezes De Oliveira, T., Mora Herrera, C., Moraes, A., Rebello Teles, P., Soeiro, M., Vilela Pereira, A., Aldá Júnior, W. L., Barroso Ferreira Filho, M., Brandao Malbouisson, H., Carvalho, W., Chinellato, J., Da Costa, E. M., Da Silveira, G. G., De Jesus Damiao, D., Fonseca De Souza, S., Gomes De Souza, R., Macedo, M., Martins, J., Mundim, L., Nogima, H., Pinheiro, J. P., Santoro, A., Sznajder, A., Thiel, M., Bernardes, C. A., Calligaris, L., Fernandez Perez Tomei, T. R., Gregores, E. M., Maietto Silverio, I., Mercadante, P. G., Novaes, S. F., Orzari, B., Padula, Sandra S., Aleksandrov, A., Antchev, G., Hadjiiska, R., Iaydjiev, P., Misheva, M., Shopova, M., Sultanov, G., Dimitrov, A., Litov, L., Pavlov, B., Petkov, P., Petrov, A., Shumka, E., Keshri, S., Laroze, D., Thakur, S., Cheng, T., Javaid, T., Yuan, L., Hu, Z., Liang, Z., Liu, J., Yi, K., Chen, G. M., Chen, H. S., Chen, M., Iemmi, F., Jiang, C. H., Kapoor, A., Liao, H., Liu, Z.-A., Sharma, R., Song, J. N., Tao, J., Wang, C., Wang, J., Wang, Z., Zhang, H., Zhao, J., Agapitos, A., Ban, Y., Deng, S., Guo, B., Jiang, C., Levin, A., Li, C., Li, Q., Mao, Y., Qian, S., Qian, S. J., Qin, X., Sun, X., Wang, D., Yang, H., Zhang, L., Zhao, Y., Zhou, C., Yang, S., You, Z., Jaffel, K., Lu, N., Bauer, G., Li, B., Zhang, J., Gao, X., Li, Y., Lin, Z., Lu, C., Xiao, M., Avila, C., Barbosa Trujillo, D. A., Cabrera, A., Florez, C., Fraga, J., Reyes Vega, J. A., Ramirez, F., Rendón, C., Rodriguez, M., Ruales Barbosa, A. A., Ruiz Alvarez, J. D., Giljanovic, D., Godinovic, N., Lelas, D., Sculac, A., Kovac, M., Petkovic, A., Sculac, T., Bargassa, P., Brigljevic, V., Chitroda, B. K., Ferencek, D., Jakovcic, K., Starodumov, A., Susa, T., Attikis, A., Christoforou, K., Hadjiagapiou, A., Leonidou, C., Mousa, J., Nicolaou, C., Paizanos, L., Ptochos, F., Razis, P. A., Rykaczewski, H., Saka, H., Stepennov, A., Finger, M., Finger, Jr., M., Kveton, A., Carrera Jarrin, E., Abdelalim, A. A., Elgammal, S., Ellithi Kamel, A., Lotfy, A., Mahmoud, M. A., Ehataht, K., Kadastik, M., Lange, T., Nandan, S., Nielsen, C., Pata, J., Raidal, M., Tani, L., Veelken, C., Kirschenmann, H., Osterberg, K., Voutilainen, M., Bharthuar, S., Bin Norjoharuddeen, N., Brücken, E., Garcia, F., Inkaew, P., Kallonen, K. T. S., Lampén, T., Lassila-Perini, K., Lehti, S., Lindén, T., Martikainen, L., Myllymäki, M., Rantanen, M. m., Siikonen, H., Tuominiemi, J., Luukka, P., Petrow, H., Besancon, M., Couderc, F., Dejardin, M., Denegri, D., Faure, J. L., Ferri, F., Ganjour, S., Gras, P., Hamel de Monchenault, G., Kumar, M., Lohezic, V., Malcles, J., Orlandi, F., Portales, L., Rosowsky, A., Sahin, M. Ö., Savoy-Navarro, A., Simkina, P., Titov, M., Tornago, M., Beaudette, F., Boldrini, G., Busson, P., Cappati, A., Charlot, C., Chiusi, M., Damas, F., Davignon, O., De Wit, A., Ehle, I. T., Fontana Santos Alves, B. A., Ghosh, S., Gilbert, A., Granier de Cassagnac, R., Hakimi, A., Harikrishnan, B., Kalipoliti, L., Liu, G., Nguyen, M., Ochando, C., Salerno, R., Sauvan, J. B., Sirois, Y., Urda Gómez, L., Vernazza, E., Zabi, A., Zghiche, A., Agram, J.-L., Andrea, J., Apparu, D., Bloch, D., Brom, J.-M., Chabert, E. C., Collard, C., Falke, S., Goerlach, U., Haeberle, R., Le Bihan, A.-C., Meena, M., Poncet, O., Saha, G., Sessini, M. A., Van Hove, P., Vaucelle, P., Di Florio, A., Amram, D., Beauceron, S., Blancon, B., Boudoul, G., Chanon, N., Contardo, D., Depasse, P., Dozen, C., El Mamouni, H., Fay, J., Gascon, S., Gouzevitch, M., Greenberg, C., Grenier, G., Ille, B., Jourd‘huy, E., Laktineh, I. B., Lethuillier, M., Mirabito, L., Perries, S., Purohit, A., Vander Donckt, M., Verdier, P., Xiao, J., Chokheli, D., Lomidze, I., Tsamalaidze, Z., Botta, V., Consuegra Rodríguez, S., Feld, L., Klein, K., Lipinski, M., Meuser, D., Pauls, A., Pérez Adán, D., Röwert, N., Teroerde, M., Diekmann, S., Dodonova, A., Eich, N., Eliseev, D., Engelke, F., Erdmann, J., Erdmann, M., Fackeldey, P., Fischer, B., Hebbeker, T., Hoepfner, K., Ivone, F., Jung, A., Lee, M. y., Mausolf, F., Merschmeyer, M., Meyer, A., Mukherjee, S., Noll, D., Nowotny, F., Pozdnyakov, A., Rath, Y., Redjeb, W., Rehm, F., Reithler, H., Sarkisovi, V., Schmidt, A., Seth, C., Sharma, A., Spah, J. L., Stein, A., Torres Da Silva De Araujo, F., Wiedenbeck, S., Zaleski, S., Dziwok, C., Flügge, G., Kress, T., Nowack, A., Pooth, O., Stahl, A., Ziemons, T., Zotz, A., Aarup Petersen, H., Aldaya Martin, M., Alimena, J., Amoroso, S., An, Y., Bach, J., Baxter, S., Bayatmakou, M., Becerril Gonzalez, H., Behnke, O., Belvedere, A., Blekman, F., Borras, K., Campbell, A., Cardini, A., Cheng, C., Colombina, F., Eckerlin, G., Eckstein, D., Estevez Banos, L. I., Filatov, O., Gallo, E., Geiser, A., Guglielmi, V., Guthoff, M., Hinzmann, A., Jeppe, L., Kaech, B., Kasemann, M., Kleinwort, C., Kogler, R., Komm, M., Krücker, D., Lange, W., Leyva Pernia, D., Lipka, K., Lohmann, W., Lorkowski, F., Mankel, R., Melzer-Pellmann, I.-A., Mendizabal Morentin, M., Meyer, A. B., Milella, G., Moral Figueroa, K., Mussgiller, A., Nair, L. P., Niedziela, J., Nürnberg, A., Otarid, Y., Park, J., Ranken, E., Raspereza, A., Rastorguev, D., Rübenach, J., Rygaard, L., Saggio, A., Scham, M., Schnake, S., Schütze, P., Schwanenberger, C., Selivanova, D., Sharko, K., Shchedrolosiev, M., Stafford, D., Vazzoler, F., Ventura Barroso, A., Walsh, R., Wang, D., Wang, Q., Wen, Y., Wichmann, K., Wiens, L., Wissing, C., Yang, Y., Zimermmane Castro Santos, A., Albrecht, A., Albrecht, S., Antonello, M., Bein, S., Benato, L., Bollweg, S., Bonanomi, M., Connor, P., El Morabit, K., Fischer, Y., Garutti, E., Grohsjean, A., Haller, J., Jabusch, H. R., Kasieczka, G., Keicher, P., Klanner, R., Korcari, W., Kramer, T., Kuo, C. c., Kutzner, V., Labe, F., Lange, J., Lobanov, A., Matthies, C., Moureaux, L., Mrowietz, M., Nigamova, A., Nissan, Y., Paasch, A., Pena Rodriguez, K. J., Quadfasel, T., Raciti, B., Rieger, M., Savoiu, D., Schindler, J., Schleper, P., Schröder, M., Schwandt, J., Sommerhalder, M., Stadie, H., Steinbrück, G., Tews, A., Wolf, M., Brommer, S., Burkart, M., Butz, E., Chwalek, T., Dierlamm, A., Droll, A., Elicabuk, U., Faltermann, N., Giffels, M., Gottmann, A., Hartmann, F., Hofsaess, R., Horzela, M., Husemann, U., Kieseler, J., Klute, M., Koppenhöfer, R., Lawhorn, J. M., Link, M., Lintuluoto, A., Maier, S., Mitra, S., Mormile, M., Müller, Th., Neukum, M., Oh, M., Pfeffer, E., Presilla, M., Quast, G., Rabbertz, K., Regnery, B., Shadskiy, N., Shvetsov, I., Simonis, H. J., Sowa, L., Stockmeier, L., Tauqeer, K., Toms, M., Trevisani, N., Von Cube, R. F., Wassmer, M., Wieland, S., Wittig, F., Wolf, R., Zuo, X., Anagnostou, G., Daskalakis, G., Kyriakis, A., Papadopoulos, A., Stakia, A., Kontaxakis, P., Melachroinos, G., Painesis, Z., Papavergou, I., Paraskevas, I., Saoulidou, N., Theofilatos, K., Tziaferi, E., Vellidis, K., Zisopoulos, I., Bakas, G., Chatzistavrou, T., Karapostoli, G., Kousouris, K., Papakrivopoulos, I., Siamarkou, E., Tsipolitis, G., Zacharopoulou, A., Adamidis, K., Bestintzanos, I., Evangelou, I., Foudas, C., Kamtsikis, C., Katsoulis, P., Kokkas, P., Kosmoglou Kioseoglou, P. G., Manthos, N., Papadopoulos, I., Strologas, J., Hajdu, C., Horvath, D., Márton, K., Rádl, A. J., Sikler, F., Veszpremi, V., Csanád, M., Farkas, K., Fehérkuti, A., Gadallah, M. M. A., Kadlecsik, Á., Major, P., Pásztor, G., Veres, G. I., Ujvari, B., Zilizi, G., Bencze, G., Czellar, S., Molnar, J., Szillasi, Z., Nemes, F., Novak, T., Bansal, S., Beri, S. B., Bhatnagar, V., Chaudhary, G., Chauhan, S., Dhingra, N., Kaur, A., Kaur, A., Kaur, H., Kaur, M., Kumar, S., Sandeep, K., Sheokand, T., Singh, J. B., Singla, A., Ahmed, A., Bhardwaj, A., Chhetri, A., Choudhary, B. C., Kumar, A., Kumar, A., Naimuddin, M., Ranjan, K., Saini, M. K., Saumya, S., Baradia, S., Barman, S., Bhattacharya, S., Das Gupta, S., Dutta, S., Dutta, S., Sarkar, S., Ameen, M. M., Behera, P. K., Behera, S. C., Chatterjee, S., Dash, G., Jana, P., Kalbhor, P., Kamble, S., Komaragiri, J. R., Kumar, D., Pujahari, P. R., Saha, N. R., Sharma, A., Sikdar, A. K., Singh, R. K., Verma, P., Verma, S., Vijay, A., Dugad, S., Mohanty, G. B., Parida, B., Shelake, M., Suryadevara, P., Bala, A., Banerjee, S., Chatterjee, R. M., Guchait, M., Jain, Sh., Jaiswal, A., Kumar, S., Majumder, G., Mazumdar, K., Parolia, S., Thachayath, A., Bahinipati, S., Kar, C., Maity, D., Mal, P., Mishra, T., Muraleedharan Nair Bindhu, V. K., Naskar, K., Nayak, A., Nayak, S., Pal, K., Sadangi, P., Swain, S. 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W., Hurtado Anampa, K., Ivanov, T., Jessop, C., Lannon, K., Lawrence, J., Loukas, N., Lutton, L., Mariano, J., Marinelli, N., Mcalister, I., McCauley, T., Mcgrady, C., Moore, C., Musienko, Y., Nelson, H., Osherson, M., Piccinelli, A., Ruchti, R., Townsend, A., Wan, Y., Wayne, M., Yockey, H., Zarucki, M., Zygala, L., Basnet, A., Bylsma, B., Carrigan, M., Durkin, L. S., Hill, C., Joyce, M., Nunez Ornelas, M., Wei, K., Winer, B. L., Yates, B. R., Bouchamaoui, H., Das, P., Dezoort, G., Elmer, P., Frankenthal, A., Greenberg, B., Haubrich, N., Kennedy, K., Kopp, G., Kwan, S., Lange, D., Loeliger, A., Marlow, D., Ojalvo, I., Olsen, J., Stickland, D., Tully, C., Malik, S., Bakshi, A. S., Chandra, S., Chawla, R., Gu, A., Gutay, L., Jones, M., Jung, A. W., Koshy, A. M., Liu, M., Negro, G., Neumeister, N., Paspalaki, G., Piperov, S., Scheurer, V., Schulte, J. F., Stojanovic, M., Thieman, J., Virdi, A. 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R., Karunarathna, N., Lee, L., Nibigira, E., Spanier, S., Aebi, D., Ahmad, M., Akhter, T., Bouhali, O., Eusebi, R., Gilmore, J., Huang, T., Kamon, T., Kim, H., Luo, S., Mueller, R., Overton, D., Rathjens, D., Safonov, A., Akchurin, N., Damgov, J., Gogate, N., Hegde, V., Hussain, A., Kazhykarim, Y., Lamichhane, K., Lee, S. W., Mankel, A., Peltola, T., Volobouev, I., Appelt, E., Chen, Y., Greene, S., Gurrola, A., Johns, W., Kunnawalkam Elayavalli, R., Melo, A., Romeo, F., Sheldon, P., Tuo, S., Velkovska, J., Viinikainen, J., Cardwell, B., Chung, H., Cox, B., Hakala, J., Hirosky, R., Ledovskoy, A., Neu, C., Bhattacharya, S., Karchin, P. E., Aravind, A., Banerjee, S., Black, K., Bose, T., Dasu, S., De Bruyn, I., Everaerts, P., Galloni, C., He, H., Herndon, M., Herve, A., Koraka, C. K., Lanaro, A., Loveless, R., Madhusudanan Sreekala, J., Mallampalli, A., Mohammadi, A., Mondal, S., Parida, G., Pétré, L., Pinna, D., Savin, A., Shang, V., Sharma, V., Smith, W. H., Teague, D., Tsoi, H. 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S., Zarubin, A., Zhizhin, I., Gavrilov, G., Golovtcov, V., Ivanov, Y., Kim, V., Levchenko, P., Murzin, V., Oreshkin, V., Sosnov, D., Sulimov, V., Uvarov, L., Vorobyev, A., Andreev, Yu., Dermenev, A., Gninenko, S., Golubev, N., Karneyeu, A., Kirpichnikov, D., Kirsanov, M., Krasnikov, N., Tlisova, I., Toropin, A., Aushev, T., Gavrilov, V., Lychkovskaya, N., Nikitenko, A., Popov, V., Zhokin, A., Chistov, R., Danilov, M., Polikarpov, S., Andreev, V., Azarkin, M., Kirakosyan, M., Terkulov, A., Boos, E., Bunichev, V., Dubinin, M., Dudko, L., Ershov, A., Gribushin, A., Klyukhin, V., Kodolova, O., Obraztsov, S., Petrushanko, S., Savrin, V., Snigirev, A., Blinov, V., Dimova, T., Kozyrev, A., Radchenko, O., Skovpen, Y., Kachanov, V., Konstantinov, D., Slabospitskii, S., Uzunian, A., Babaev, A., Borshch, V., Druzhkin, D., Chekhovsky, V., and Makarenko, V.
Published: 2024
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49. Search for a resonance decaying to a W boson and a photon in proton-proton collisions at s = 13 TeV using leptonic W boson decays

Author: Hayrapetyan, A., Tumasyan, A., Adam, W., Andrejkovic, J. W., Bergauer, T., Chatterjee, S., Damanakis, K., Dragicevic, M., Hussain, P. S., Jeitler, M., Krammer, N., Li, A., Liko, D., Mikulec, I., Schieck, J., Schöfbeck, R., Schwarz, D., Sonawane, M., Templ, S., Waltenberger, W., Wulz, C.-E., Janssen, T., Van Laer, T., Van Mechelen, P., Breugelmans, N., D’Hondt, J., Dansana, S., De Moor, A., Delcourt, M., Heyen, F., Lowette, S., Makarenko, I., Müller, D., Tavernier, S., Tytgat, M., Van Onsem, G. P., Van Putte, S., Vannerom, D., Bilin, B., Clerbaux, B., Das, A. K., De Lentdecker, G., Evard, H., Favart, L., Gianneios, P., Jaramillo, J., Khalilzadeh, A., Khan, F. A., Lee, K., Mahdavikhorrami, M., Malara, A., Paredes, S., Shahzad, M. A., Thomas, L., Vanden Bemden, M., Vander Velde, C., Vanlaer, P., De Coen, M., Dobur, D., Gokbulut, G., Hong, Y., Knolle, J., Lambrecht, L., Marckx, D., Mota Amarilo, K., Samalan, A., Skovpen, K., Van Den Bossche, N., van der Linden, J., Wezenbeek, L., Benecke, A., Bethani, A., Bruno, G., Caputo, C., De Favereau De Jeneret, J., Delaere, C., Donertas, I. S., Giammanco, A., Guzel, A. O., Jain, Sa., Lemaitre, V., Lidrych, J., Mastrapasqua, P., Tran, T. T., Wertz, S., Alves, G. A., Alves Gallo Pereira, M., Coelho, E., Correia Silva, G., Hensel, C., Menezes De Oliveira, T., Mora Herrera, C., Moraes, A., Rebello Teles, P., Soeiro, M., Vilela Pereira, A., Aldá Júnior, W. L., Barroso Ferreira Filho, M., Brandao Malbouisson, H., Carvalho, W., Chinellato, J., Da Costa, E. M., Da Silveira, G. G., De Jesus Damiao, D., Fonseca De Souza, S., Gomes De Souza, R., Macedo, M., Martins, J., Mundim, L., Nogima, H., Pinheiro, J. P., Santoro, A., Sznajder, A., Thiel, M., Bernardes, C. A., Calligaris, L., Fernandez Perez Tomei, T. R., Gregores, E. M., Lopes Da Costa, B., Maietto Silverio, I., Mercadante, P. G., Novaes, S. F., Orzari, B., Padula, Sandra S., Aleksandrov, A., Antchev, G., Hadjiiska, R., Iaydjiev, P., Misheva, M., Shopova, M., Sultanov, G., Dimitrov, A., Litov, L., Pavlov, B., Petkov, P., Petrov, A., Shumka, E., Keshri, S., Laroze, D., Thakur, S., Cheng, T., Javaid, T., Yuan, L., Hu, Z., Liang, Z., Liu, J., Yi, K., Chen, G. M., Chen, H. S., Chen, M., Iemmi, F., Jiang, C. H., Kapoor, A., Liao, H., Liu, Z.-A., Sharma, R., Song, J. N., Tao, J., Wang, C., Wang, J., Wang, Z., Zhang, H., Zhao, J., Agapitos, A., Ban, Y., Deng, S., Guo, B., Jiang, C., Levin, A., Li, C., Li, Q., Mao, Y., Qian, S., Qian, S. J., Qin, X., Sun, X., Wang, D., Yang, H., Zhang, L., Zhao, Y., Zhou, C., Yang, S., You, Z., Jaffel, K., Lu, N., Bauer, G., Li, B., Zhang, J., Gao, X., Li, Y., Lin, Z., Lu, C., Xiao, M., Avila, C., Barbosa Trujillo, D. A., Cabrera, A., Florez, C., Fraga, J., Reyes Vega, J. A., Ramirez, F., Rendón, C., Rodriguez, M., Ruales Barbosa, A. A., Ruiz Alvarez, J. D., Giljanovic, D., Godinovic, N., Lelas, D., Sculac, A., Kovac, M., Petkovic, A., Sculac, T., Bargassa, P., Brigljevic, V., Chitroda, B. K., Ferencek, D., Jakovcic, K., Mishra, S., Starodumov, A., Susa, T., Attikis, A., Christoforou, K., Hadjiagapiou, A., Leonidou, C., Mousa, J., Nicolaou, C., Paizanos, L., Ptochos, F., Razis, P. A., Rykaczewski, H., Saka, H., Stepennov, A., Finger, M., Finger, Jr., M., Kveton, A., Carrera Jarrin, E., Assran, Y., El-mahdy, B., Elgammal, S., Mahmoud, M. A., Mohammed, Y., Ehataht, K., Kadastik, M., Lange, T., Nandan, S., Nielsen, C., Pata, J., Raidal, M., Tani, L., Veelken, C., Kirschenmann, H., Osterberg, K., Voutilainen, M., Bharthuar, S., Bin Norjoharuddeen, N., Brücken, E., Garcia, F., Inkaew, P., Kallonen, K. T. S., Lampén, T., Lassila-Perini, K., Lehti, S., Lindén, T., Martikainen, L., Myllymäki, M., Rantanen, M. m., Siikonen, H., Tuominiemi, J., Luukka, P., Petrow, H., Besancon, M., Couderc, F., Dejardin, M., Denegri, D., Faure, J. L., Ferri, F., Ganjour, S., Gras, P., Hamel de Monchenault, G., Kumar, M., Lohezic, V., Malcles, J., Orlandi, F., Portales, L., Rosowsky, A., Sahin, M. Ö., Savoy-Navarro, A., Simkina, P., Titov, M., Tornago, M., Beaudette, F., Boldrini, G., Busson, P., Cappati, A., Charlot, C., Chiusi, M., Damas, F., Davignon, O., De Wit, A., Ehle, I. T., Fontana Santos Alves, B. A., Ghosh, S., Gilbert, A., Granier de Cassagnac, R., Hakimi, A., Harikrishnan, B., Kalipoliti, L., Liu, G., Nguyen, M., Ochando, C., Salerno, R., Sauvan, J. B., Sirois, Y., Urda Gómez, L., Vernazza, E., Zabi, A., Zghiche, A., Agram, J.-L., Andrea, J., Apparu, D., Bloch, D., Brom, J.-M., Chabert, E. C., Collard, C., Falke, S., Goerlach, U., Haeberle, R., Le Bihan, A.-C., Meena, M., Poncet, O., Saha, G., Sessini, M. A., Van Hove, P., Vaucelle, P., Di Florio, A., Amram, D., Beauceron, S., Blancon, B., Boudoul, G., Chanon, N., Contardo, D., Depasse, P., Dozen, C., El Mamouni, H., Fay, J., Gascon, S., Gouzevitch, M., Greenberg, C., Grenier, G., Ille, B., Jourd‘huy, E., Laktineh, I. B., Lethuillier, M., Mirabito, L., Perries, S., Purohit, A., Vander Donckt, M., Verdier, P., Xiao, J., Bagaturia, I., Lomidze, I., Tsamalaidze, Z., Botta, V., Consuegra Rodríguez, S., Feld, L., Klein, K., Lipinski, M., Meuser, D., Pauls, A., Pérez Adán, D., Röwert, N., Teroerde, M., Diekmann, S., Dodonova, A., Eich, N., Eliseev, D., Engelke, F., Erdmann, J., Erdmann, M., Fackeldey, P., Fischer, B., Hebbeker, T., Hoepfner, K., Ivone, F., Jung, A., Lee, M. y., Mausolf, F., Merschmeyer, M., Meyer, A., Mukherjee, S., Noll, D., Nowotny, F., Pozdnyakov, A., Rath, Y., Redjeb, W., Rehm, F., Reithler, H., Sarkisovi, V., Schmidt, A., Seth, C., Sharma, A., Spah, J. L., Stein, A., Torres Da Silva De Araujo, F., Wiedenbeck, S., Zaleski, S., Dziwok, C., Flügge, G., Kress, T., Nowack, A., Pooth, O., Stahl, A., Ziemons, T., Zotz, A., Aarup Petersen, H., Aldaya Martin, M., Alimena, J., Amoroso, S., An, Y., Bach, J., Baxter, S., Bayatmakou, M., Becerril Gonzalez, H., Behnke, O., Belvedere, A., Blekman, F., Borras, K., Campbell, A., Cardini, A., Cheng, C., Colombina, F., De Silva, M., Eckerlin, G., Eckstein, D., Estevez Banos, L. I., Filatov, O., Gallo, E., Geiser, A., Guglielmi, V., Guthoff, M., Hinzmann, A., Jeppe, L., Kaech, B., Kasemann, M., Kleinwort, C., Kogler, R., Komm, M., Krücker, D., Lange, W., Leyva Pernia, D., Lipka, K., Lohmann, W., Lorkowski, F., Mankel, R., Melzer-Pellmann, I.-A., Mendizabal Morentin, M., Meyer, A. B., Milella, G., Moral Figueroa, K., Mussgiller, A., Nair, L. P., Niedziela, J., Nürnberg, A., Otarid, Y., Park, J., Ranken, E., Raspereza, A., Rastorguev, D., Rübenach, J., Rygaard, L., Saggio, A., Scham, M., Schnake, S., Schütze, P., Schwanenberger, C., Selivanova, D., Sharko, K., Shchedrolosiev, M., Stafford, D., Vazzoler, F., Ventura Barroso, A., Walsh, R., Wang, D., Wang, Q., Wen, Y., Wichmann, K., Wiens, L., Wissing, C., Yang, Y., Zimermmane Castro Santos, A., Albrecht, A., Albrecht, S., Antonello, M., Bein, S., Benato, L., Bollweg, S., Bonanomi, M., Connor, P., El Morabit, K., Fischer, Y., Garutti, E., Grohsjean, A., Haller, J., Jabusch, H. R., Kasieczka, G., Keicher, P., Klanner, R., Korcari, W., Kramer, T., Kuo, C. c., Kutzner, V., Labe, F., Lange, J., Lobanov, A., Matthies, C., Moureaux, L., Mrowietz, M., Nigamova, A., Nissan, Y., Paasch, A., Pena Rodriguez, K. J., Quadfasel, T., Raciti, B., Rieger, M., Savoiu, D., Schindler, J., Schleper, P., Schröder, M., Schwandt, J., Sommerhalder, M., Stadie, H., Steinbrück, G., Tews, A., Wolf, M., Brommer, S., Burkart, M., Butz, E., Chwalek, T., Dierlamm, A., Droll, A., Elicabuk, U., Faltermann, N., Giffels, M., Gottmann, A., Hartmann, F., Hofsaess, R., Horzela, M., Husemann, U., Kieseler, J., Klute, M., Koppenhöfer, R., Lawhorn, J. M., Link, M., Lintuluoto, A., Maier, B., Maier, S., Mitra, S., Mormile, M., Müller, Th., Neukum, M., Oh, M., Pfeffer, E., Presilla, M., Quast, G., Rabbertz, K., Regnery, B., Shadskiy, N., Shvetsov, I., Simonis, H. J., Sowa, L., Stockmeier, L., Tauqeer, K., Toms, M., Trevisani, N., Von Cube, R. 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F., Vetens, W., Warden, A., Afanasiev, S., Alexakhin, V., Andreev, V., Andreev, Yu., Aushev, T., Azarkin, M., Babaev, A., Blinov, V., Boos, E., Borshch, V., Budkouski, D., Bunichev, V., Chekhovsky, V., Chistov, R., Danilov, M., Dermenev, A., Dimova, T., Druzhkin, D., Dubinin, M., Dudko, L., Gavrilov, G., Gavrilov, V., Gninenko, S., Golovtcov, V., Golubev, N., Golutvin, I., Gorbunov, I., Gribushin, A., Ivanov, Y., Kachanov, V., Karjavine, V., Karneyeu, A., Kim, V., Kirakosyan, M., Kirpichnikov, D., Kirsanov, M., Klyukhin, V., Kodolova, O., Konstantinov, D., Korenkov, V., Kozyrev, A., Krasnikov, N., Lanev, A., Levchenko, P., Lychkovskaya, N., Makarenko, V., Malakhov, A., Matveev, V., Murzin, V., Nikitenko, A., Obraztsov, S., Oreshkin, V., Palichik, V., Perelygin, V., Perfilov, M., Petrushanko, S., Polikarpov, S., Popov, V., Radchenko, O., Savina, M., Savrin, V., Shalaev, V., Shmatov, S., Shulha, S., Skovpen, Y., Slabospitskii, S., Smirnov, V., Sosnov, D., Sulimov, V., Terkulov, A., Teryaev, O., Tlisova, I., Toropin, A., Uvarov, L., Uzunian, A., Vorobyev, A., Vorotnikov, G., Voytishin, N., Yuldashev, B. S., Zarubin, A., Zhizhin, I., and Zhokin, A.
Published: 2024
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50. The Impact of Cytomegalovirus Infection on Ulcerative Colitis Relapse: A Multicenter Retrospective Cohort Study

Author: Xiao L, Ma J, Chen R, Chen J, Wang Q, Tang N, Zhao X, Zhang H, and Jiao C
Subjects: ulcerative colitis, cytomegalovirus colitis, relapse, risk factors, Pathology, RB1-214, Therapeutics. Pharmacology, RM1-950
Abstract: Linmei Xiao,1,&ast; Jingjing Ma,2,&ast; Ruidong Chen,2,3,&ast; Jie Chen,4 Qiang Wang,5 Nana Tang,2 Xiaojing Zhao,2 Hongjie Zhang,2 Chunhua Jiao2 1Department of Liver Disease, Wuxi No.5 People’s Hospital Affiliated to Jiangnan University, Wuxi, People’s Republic of China; 2Department of Gastroenterology, The First Affiliated Hospital with Nanjing Medical University, Nanjing, Jiangsu Province, People’s Republic of China; 3Department of Gastroenterology, The Second Affiliated Hospital of Soochow University, Suzhou, People’s Republic of China; 4Northern Jiangsu People’s Hospital/Northern Jiangsu People’s Hospital of Jiangsu Province, Yangzhou, Jiangsu Province, People’s Republic of China; 5Jiangsu Shengze Hospital, Suzhou, Jiangsu Province, People’s Republic of China&ast;These authors contributed equally to this workCorrespondence: Chunhua Jiao; Hongjie Zhang, The First Affiliated Hospital of Nanjing Medical University, 300 Guangzhou Road, Nanjing, Jiangsu Province, 210029, People’s Republic of China, Tel +86 13913928581, Email jch0409@163.com; hjzhang06@163.comPurpose: Cytomegalovirus (CMV) infection exacerbates intestinal inflammation in ulcerative colitis (UC) patients, yet the effect of CMV infection on UC relapse has not been fully elucidated. This study aimed to investigate the impact of CMV infection on UC relapse and identify associated risk factors.Patients and Methods: This multicenter retrospective cohort study included UC patients who visited research centers from January 2016 to December 2020. Univariate and multivariate Cox regression analyses were conducted to explore risk factors for UC relapse. Propensity score matching was used to balance the differences in the clinical characteristics between the groups.Results: A total of 298 UC patients participated in this study, including 19 with CMV colitis, 37 with CMV viremia, and 242 CMV-negative patients. The 2-year cumulative recurrence rate was higher in patients with CMV colitis than that in CMV-negative patients (84.21% vs 51.65%, p = 0.01). Univariate and multivariate Cox regression analyses confirmed that fecal calprotectin ≥ 250 μg/g, Montreal classification E3, CMV colitis, duration > 48 months, and serum albumin < 30 g/L were independent risk factors for UC relapse at 2 years, whereas the use of biologics for induction of remission was identified as an independent protective factor.Conclusion: Our study suggests that the risk of relapse increases among UC patients with CMV colitis over two years. Risk factors for UC relapse at 2 years include fecal calprotectin ≥ 250 μg/g, Montreal classification E3, CMV colitis, UC duration > 48 months, and albumin < 30 g/L, whereas the use of biologics during induction is a protective factor.Plain Language Summary: Patients with ulcerative colitis and cytomegalovirus colitis are at a higher risk of relapse over a 2-year period than those who are CMV negative. Additionally, we identified several risk factors for UC relapse at 2 years, including fecal calprotectin ≥ 250 μg/g, Montreal classification E3, CMV colitis, duration of UC ≥ 48 months, and albumin < 30 g/L, whereas the administration of biologics during remission induction contributed to reducing UC relapse.Keywords: Ulcerative colitis, cytomegalovirus colitis, relapse, risk factors
Published: 2024

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