First Dark Matter Search Results from the LUX-ZEPLIN (LZ) Experiment

Aalbers, J.; Akerib, D. S.; Akerlof, C. W.; Musalhi, A. K. Al; Alder, F.; Alqahtani, A.; Alsum, S. K.; Amarasinghe, C. S.; Ames, A.; Anderson, T. J.; Angelides, N.; Araújo, H. M.; Armstrong, J. E.; Arthurs, M.; Azadi, S.; Bailey, A. J.; Baker, A.; Balajthy, J.; Balashov, S.; Bang, J.; Bargemann, J. W.; Barry, M. J.; Barthel, J.; Bauer, D.; Baxter, A.; Beattie, K.; Belle, J.; Beltrame, P.; Bensinger, J.; Benson, T.; Bernard, E. P.; Bhatti, A.; Biekert, A.; Biesiadzinski, T. P.; Birch, H. J.; Birrittella, B.; Blockinger, G. M.; Boast, K. E.; Boxer, B.; Bramante, R.; Brew, C. A. J.; Brás, P.; Buckley, J. H.; Bugaev, V. V.; Burdin, S.; Busenitz, J. K.; Buuck, M.; Cabrita, R.; Carels, C.; Carlsmith, D. L.; Carlson, B.; Carmona-Benitez, M. C.; Cascella, M.; Chan, C.; Chawla, A.; Chen, H.; Cherwinka, J. J.; Chott, N. I.; Cole, A.; Coleman, J.; Converse, M. V.; Cottle, A.; Cox, G.; Craddock, W. W.; Creaner, O.; Curran, D.; Currie, A.; Cutter, J. E.; Dahl, C. E.; David, A.; Davis, J.; Davison, T. J. R.; Delgaudio, J.; Dey, S.; de Viveiros, L.; Dobi, A.; Dobson, J. E. Y.; Druszkiewicz, E.; Dushkin, A.; Edberg, T. K.; Edwards, W. R.; Elnimr, M. M.; Emmet, W. T.; Eriksen, S. R.; Faham, C. H.; Fan, A.; Fayer, S.; Fearon, N. M.; Fiorucci, S.; Flaecher, H.; Ford, P.; Francis, V. B.; Fraser, E. D.; Fruth, T.; Gaitskell, R. J.; Gantos, N. J.; Garcia, D.; Geffre, A.; Gehman, V. M.; Genovesi, J.; Ghag, C.; Gibbons, R.; Gibson, E.; Gilchriese, M. G. D.; Gokhale, S.; Gomber, B.; Green, J.; Greenall, A.; Greenwood, S.; van der Grinten, M. G. D.; Gwilliam, C. B.; Hall, C. R.; Hans, S.; Hanzel, K.; Harrison, A.; Hartigan-O'Connor, E.; Haselschwardt, S. J.; Hertel, S. A.; Heuermann, G.; Hjemfelt, C.; Hoff, M. D.; Holtom, E.; Hor, J. Y-K.; Horn, M.; Huang, D. Q.; Hunt, D.; Ignarra, C. M.; Jacobsen, R. G.; Jahangir, O.; James, R. S.; Jeffery, S. N.; Ji, W.; Johnson, J.; Kaboth, A. C.; Kamaha, A. C.; Kamdin, K.; Kasey, V.; Kazkaz, K.; Keefner, J.; Khaitan, D.; Khaleeq, M.; Khazov, A.; Khurana, I.; Kim, Y. D.; Kocher, C. D.; Kodroff, D.; Korley, L.; Korolkova, E. V.; Kras, J.; Kraus, H.; Kravitz, S.; Krebs, H. J.; Kreczko, L.; Krikler, B.; Kudryavtsev, V. A.; Kyre, S.; Landerud, B.; Leason, E. A.; Lee, C.; Lee, J.; Leonard, D. S.; Leonard, R.; Lesko, K. T.; Levy, C.; Li, J.; Liao, F. -T.; Liao, J.; Lin, J.; Lindote, A.; Linehan, R.; Lippincott, W. H.; Liu, R.; Liu, X.; Liu, Y.; Loniewski, C.; Lopes, M. I.; Asamar, E. Lopez; Paredes, B. López; Lorenzon, W.; Lucero, D.; Luitz, S.; Lyle, J. M.; Majewski, P. A.; Makkinje, J.; Malling, D. C.; Manalaysay, A.; Manenti, L.; Mannino, R. L.; Marangou, N.; Marzioni, M. F.; Maupin, C.; McCarthy, M. E.; McConnell, C. T.; McKinsey, D. N.; McLaughlin, J.; Meng, Y.; Migneault, J.; Miller, E. H.; Mizrachi, E.; Mock, J. A.; Monte, A.; Monzani, M. E.; Morad, J. A.; Mendoza, J. D. Morales; Morrison, E.; Mount, B. J.; Murdy, M.; Murphy, A. St. J.; Naim, D.; Naylor, A.; Nedlik, C.; Nehrkorn, C.; Nelson, H. N.; Neves, F.; Nguyen, A.; Nikoleyczik, J. A.; Nilima, A.; O'Dell, J.; O'Neill, F. G.; O'Sullivan, K.; Olcina, I.; Olevitch, M. A.; Oliver-Mallory, K. C.; Orpwood, J.; Pagenkopf, D.; Pal, S.; Palladino, K. J.; Palmer, J.; Pangilinan, M.; Parveen, N.; Patton, S. J.; Pease, E. K.; Penning, B.; Pereira, C.; Pereira, G.; Perry, E.; Pershing, T.; Peterson, I. B.; Piepke, A.; Podczerwinski, J.; Porzio, D.; Powell, S.; Preece, R. M.; Pushkin, K.; Qie, Y.; Ratcliff, B. N.; Reichenbacher, J.; Reichhart, L.; Rhyne, C. A.; Richards, A.; Riffard, Q.; Rischbieter, G. R. C.; Rodrigues, J. P.; Rodriguez, A.; Rose, H. J.; Rosero, R.; Rossiter, P.; Rushton, T.; Rutherford, G.; Rynders, D.; Saba, J. S.; Santone, D.; Sazzad, A. B. M. R.; Schnee, R. W.; Scovell, P. R.; Seymour, D.; Shaw, S.; Shutt, T.; Silk, J. J.; Silva, C.; Sinev, G.; Skarpaas, K.; Skulski, W.; Smith, R.; Solmaz, M.; Solovov, V. N.; Sorensen, P.; Soria, J.; Stancu, I.; Stark, M. R.; Stevens, A.; Stiegler, T. M.; Stifter, K.; Studley, R.; Suerfu, B.; Sumner, T. J.; Sutcliffe, P.; Swanson, N.; Szydagis, M.; Tan, M.; Taylor, D. J.; Taylor, R.; Taylor, W. C.; Temples, D. J.; Tennyson, B. P.; Terman, P. A.; Thomas, K. J.; Tiedt, D. R.; Timalsina, M.; To, W. H.; Tomás, A.; Tong, Z.; Tovey, D. R.; Tranter, J.; Trask, M.; Tripathi, M.; Tronstad, D. R.; Tull, C. E.; Turner, W.; Tvrznikova, L.; Utku, U.; Va'vra, J.; Vacheret, A.; Vaitkus, A. C.; Verbus, J. R.; Voirin, E.; Waldron, W. L.; Wang, A.; Wang, B.; Wang, J. J.; Wang, W.; Wang, Y.; Watson, J. R.; Webb, R. C.; White, A.; White, D. T.; White, J. T.; White, R. G.; Whitis, T. J.; Williams, M.; Wisniewski, W. J.; Witherell, M. S.; Wolfs, F. L. H.; Wolfs, J. D.; Woodford, S.; Woodward, D.; Worm, S. D.; Wright, C. J.; Xia, Q.; Xiang, X.; Xiao, Q.; Xu, J.; Yeh, M.; Yin, J.; Young, I.; Zarzhitsky, P.; Zuckerman, A.; Zweig, E. A.

doi:10.48550/arxiv.2207.03764

Cited by 82 publications

(148 citation statements)

References 78 publications

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“…4) Particle physics point of view, no single known particle can be considered as a dark matter candidate. 5) So far, no ground based experiment or no cosmological observation could establish any direct evidence for the existence of dark matter [5,6,7]. 6) To some extent, existence of dark matter can be confirmed with confirming the existence of 'pure dark matter' galaxies (galaxies having no baryonic matter).…”

Section: Dark Matter As a Super Gravity Of Baryonic Mass Of Galaxymentioning

confidence: 99%

“…In case of dark matter deficient galaxies, the basic question to be answered is, why mother galaxy is absorbing dwarf galaxy's dark matter in larger proportion compared to dwarf galaxy's baryonic matter? To understand this issue, scientists are developing 'self interacting' dark matter models [5]. Compared to 'tidal stripping' and 'self interacting' mechanisms, our approach is very simple in understanding the deficiency of galactic dark matter.…”

Section: Dark Matter As a Super Gravity Of Baryonic Mass Of Galaxymentioning

confidence: 99%

“…To understand the absence of dark matter in dwarf galaxies, 'tidal stripping' and 'self interacting dark matter' models have been introduced [2,3,4]. Most recent and most advanced experiments like Lux-Zeplin and ORGAN are showing their inability in detecting weakly interacting massive particles and axions like very light particles [5,6,7]. Experimentalists are trying to tune the experimental set up for detecting dark matter particles in various mass ranges.…”

Section: Introductionmentioning

confidence: 99%

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Weak Interaction Dependent Super Gravity of Galactic Baryon Mass

U.V¹,

S²

2022

Preprint

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In our recently published papers, considering Planck mass based light speed growing black hole universe and scaled Hawking’s black hole temperature formula, we have developed a simple procedure for estimating the current Hubble parameter and current cosmic mass. In addition to that, without considering galactic dark matter, starting from 10 km/sec to 500 km/sec, we have tried to fit the observed galactic flat rotation speeds with a concept of super gravity of galactic baryonic mass. To estimate the equivalent mass of currently hypothecated galactic dark matter, we have introduced a timely increasing cosmological reference mass unit. Its current magnitude seems to be around 200 million solar masses. In this paper, considering 200 million solar masses as a characteristic representation of cosmic weak interaction mass unit, we have developed a simple formula for its estimation. We would like to appeal that, weak interaction boosts the gravity of galaxies in proportion with their virtual dark mass as (galactic baryonic mass)3/2 / (200 million solar masses)1/2. With further study- dark matter existence and physical properties can be understood in a theoretical approach.

show abstract

Section: Dark Matter As a Super Gravity Of Baryonic Mass Of Galaxymentioning

confidence: 99%

Section: Dark Matter As a Super Gravity Of Baryonic Mass Of Galaxymentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Weak Interaction Dependent Super Gravity of Galactic Baryon Mass

U.V¹,

S²

2022

Preprint

View full text Add to dashboard Cite

show abstract

“…Typically weak couplings and DM masses near the weak scale are required for this. Motivated in part by the lack of conclusive evidence for such WIMPs despite the extensive astrophysical and colliders search program underway [2,3,4,5], recently a much larger range of DM masses and couplings have been explored, and different mechanisms for DM formation have been proposed.…”

Section: Introductionmentioning

confidence: 99%

Co-scattering in micrOMEGAs: a case study for the singlet-triplet dark matter model

Alguero¹,

Bélanger²,

Kraml³

et al. 2022

Preprint

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In scenarios with very small dark matter (DM) couplings and small mass splittings between the DM and other dark sector particles, so-called "co-scattering" or "conversion-driven freeze-out" can be the dominant mechanism for DM production. We present the inclusion of this mechanism in micrOMEGAs together with a case study of the phenomenological implications in the fermionic singlet-triplet model. For the latter, we focus on the transition between co-annihilation and co-scattering processes. We observe that co-scattering is needed to describe the thermal behaviour of the DM for very small couplings, opening up a new region in the parameter space of the model. The triplet states are often long-lived in this region; we therefore also discuss LHC constraints from long-lived signatures obtained with SModelS.

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“…Despite plenty of astrophysical evidence of DM existence in the Universe, however, the constitution and the properties of DM are still mystery. Up to now, there is no conclusive evidence of the weakly interacting massive particle (WIMP) in DM direct detection (DD) experiments [1,2]. Much more effort has recently been paid to the theoretical hypotheses beyond the WIMP and their detection methods in experiments.…”

Section: Introductionmentioning

confidence: 99%

Axion-like particles from primordial black hole evaporation and their detection in neutrino experiments

Li¹,

Zhang²

2022

Preprint

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The primordial black holes (PBHs) play as a novel source to radiate light elementary particles of energies in the region of a few hundred MeV. We explore the possibility that the axion-like particles (ALPs) with mass less than 1 MeV are produced from PBH evaporation. The absorption of light ALPs in the underground detector targets then induces energetic photoelectron signatures in current and future neutrino experiments.Utilizing the PBH ALP event rate, we place general exclusion limits on the axion couplings at Super-K and Hyper-K. We also translate these limits into the upper bound on the fraction of DM composed of PBHs f PBH .

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First Dark Matter Search Results from the LUX-ZEPLIN (LZ) Experiment

Cited by 82 publications

References 78 publications

Weak Interaction Dependent Super Gravity of Galactic Baryon Mass

Weak Interaction Dependent Super Gravity of Galactic Baryon Mass

Co-scattering in micrOMEGAs: a case study for the singlet-triplet dark matter model

Axion-like particles from primordial black hole evaporation and their detection in neutrino experiments

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