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3. 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

4. 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

5. 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

6. 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

7. 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

8. 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

9. 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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10. 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

11. 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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12. 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

13. 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

14. 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

15. 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

16. 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

17. 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

18. 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

19. 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

21. 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

22. 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

23. 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

24. 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

25. 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

26. 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

27. 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

28. 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

29. 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

30. 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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31. 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

32. 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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33. 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

34. 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

39. Detailed study of a rare hyperluminous rotating disk in an Einstein ring 10 billion years ago

Author

Liu, Daizhong, Förster Schreiber, Natascha M., Harrington, Kevin C., Lee, Lilian L., Kamieneski, Patrick S., Davies, Richard I., Lutz, Dieter, Renzini, Alvio, Wuyts, Stijn, Tacconi, Linda J., Genzel, Reinhard, Burkert, Andreas, Herrera-Camus, Rodrigo, Alcalde Pampliega, Belén, Vishwas, Amit, Kaasinen, Melanie, Wang, Q. Daniel, Jiménez-Andrade, Eric F., Lowenthal, James, Foo, Nicholas, Frye, Brenda L., Shangguan, Jinyi, Cao, Yixian, Agapito, Guido, Berbel, Alex Agudo, Barfety, Capucine, Baruffolo, Andrea, Berman, Derek, Black, Martin, Bonaglia, Marco, Briguglio, Runa, Carbonaro, Luca, Chapman, Lee, Chen, Jianhang, Cikota, Aleksandar, Concas, Alice, Cooper, Olivia, Cresci, Giovanni, Dallilar, Yigit, Deysenroth, Matthias, Di Antonio, Ivan, Di Cianno, Amico, Di Rico, Gianluca, Doelman, David, Dolci, Mauro, Eisenhauer, Frank, Espejo, Juan, Esposito, Simone, Fantinel, Daniela, Ferruzzi, Debora, Feuchtgruber, Helmut, Gao, Xiaofeng, Garcia Diaz, Carlos, Gillessen, Stefan, Grani, Paolo, Hartl, Michael, Henry, David, Huber, Heinrich, Jolly, Jean-Baptiste, Keller, Christoph U., Kenworthy, Matthew, Kravchenko, Kateryna, Lee, Minju M., Lightfoot, John, Lunney, David, Macintosh, Mike, Mannucci, Filippo, Ott, Thomas, Pascale, Massimo, Pastras, Stavros, Pearson, David, Puglisi, Alfio, Pulsoni, Claudia, Rabien, Sebastian, Rau, Christian, Riccardi, Armando, Salasnich, Bernardo, Shimizu, Taro, Snik, Frans, Sturm, Eckhard, Taylor, William, Valentini, Angelo, Waring, Christopher, Wiezorrek, Erich, Xompero, Marco, and Yun, Min S.

Published
2024
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43. 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.

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2024
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44. Observation of the Λb0→J/ψΞ-K+ decay

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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. 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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. 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S., Zarubin, A., Zhizhin, I., and Zhokin, A.

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2024
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45. Search for Higgs boson pair production with one associated vector boson in proton-proton collisions at s = 13 TeV

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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. 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., Lotfy, A., Mahmoud, M. A., 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., 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. 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. 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S., Zarubin, A., Zhizhin, I., and Zhokin, A.

Published
2024
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46. 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

47. 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

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