View source for Organization:LZ experiment

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| name                    = LUX-Zeplin (LZ) experiment
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| image_skyline           = LUX-Zeplin -LZ- experiment, an international collaboration, is a WIMP- detector managed by Berkeley Lab and to be located in South Dakota.jpg
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| website                 = [http://lz.lbl.gov/ The LZ Dark Matter Experiment]
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The '''LUX-ZEPLIN (LZ) Experiment''' is a next-generation dark matter direct detection experiment hoping to observe [[Physics:Weakly interacting massive particles|weakly interacting massive particles]] (WIMP) scatters on nuclei.<ref>{{cite web | last = Toomey | first = Emily | title = New Generation of Dark Matter Experiments Gear Up to Search for Elusive Particle | website = Smithsonian Magazine | url = https://www.smithsonianmag.com/science-nature/new-generation-dark-matter-experiments-gear-search-elusive-particle-180974111/ | date = 3 February 2020 | access-date = 11 April 2021}}</ref> It was formed in 2012 by combining the [[Physics:Large Underground Xenon experiment|LUX]] and [[Physics:ZEPLIN-III|ZEPLIN]] groups. It is currently a collaboration of 30 institutes in the US, UK, Portugal and {{wipe|South Korea}}. The experiment is located at the [[Organization:Sanford Underground Research Facility|Sanford Underground Research Facility]] (SURF) in South Dakota,<ref>[http://www.higheredjobs.com/m/details.cfm?JobCode=175986353&Title=LZ%20Lab%20Technician%20(Materials%20Laboratory%20Technician) LZ Lab Technician (Materials Laboratory Technician)] HigherJobEd of "South Dakota School of Mines and Technology"</ref> and is managed by the United States Department of Energy's (DOE) Lawrence Berkeley National Lab (Berkeley Lab). 

The experiment uses an ultra-sensitive detector made of 7 tonnes of liquid xenon to hunt for signals of WIMP-nucleus interactions. It is one of three such experiments which lead the search for direct detection of WIMPs above 10 GeV/c<sup>2</sup>, the other two being the [[Physics:XENON|XENONnT]] experiment and the [[Astronomy:PandaX|PANDAX]]-4T experiment. 

In the spring of 2015, LZ passed the "Critical Decision Step 1" or CD-1 review, and became an official DOE project.<ref>[http://lz.lbl.gov/ Welcome to the LZ dark matter experiment's webpage]</ref> U.S. Department of Energy officials on Sept. 21, 2020 formally signed off on project completion for LZ; DOE's project completion milestone is called Critical Decision 4, or CD-4.<ref>{{Cite web|url=https://www.sanfordlab.org/article/major-milestone-underground-dark-matter-search-experiment|title = A major milestone for an underground dark matter search experiment}}</ref>
== LZ as a low-background detector ==
{{Unsourced section|date=July 2022}}
To conclusively identify WIMP-nucleus scatters, LZ must be able to observe very small energy depositions in its active volume. However, it must also be able to differentiate true WIMP scatters from other interactions caused by known particles. Examples of these known "backgrounds" are interactions from [[Physics:Gamma ray|gamma rays]] produced by trace radioactivity in the environment, interactions from [[Physics:Neutron|neutrons]] produced in the environment, and interactions from cosmic ray [[Physics:Muon|muons]] produced in the upper atmosphere. The two goals of a dark matter search are to minimize the number of these background interactions, and for those that do occur, to be able to identify that they are from background (as opposed to WIMPs).

First, the innermost detector is composed of a dual-phase [[Chemistry:Xenon|xenon]] [[Physics:Time projection chamber|time projection chamber (TPC)]].<ref>{{Cite journal|title = The LUX-ZEPLIN (LZ) experiment| year=2020 | doi=10.1016/j.nima.2019.163047 | arxiv=1910.09124 | last1=Akerib | first1=D.S. | last2=Akerlof | first2=C.W. | last3=Akimov | first3=D.Yu. | last4=Alquahtani | first4=A. | last5=Alsum | first5=S.K. | last6=Anderson | first6=T.J. | last7=Angelides | first7=N. | last8=Araújo | first8=H.M. | last9=Arbuckle | first9=A. | last10=Armstrong | first10=J.E. | last11=Arthurs | first11=M. | last12=Auyeung | first12=H. | last13=Bai | first13=X. | last14=Bailey | first14=A.J. | last15=Balajthy | first15=J. | last16=Balashov | first16=S. | last17=Bang | first17=J. | last18=Barry | first18=M.J. | last19=Barthel | first19=J. | last20=Bauer | first20=D. | last21=Bauer | first21=P. | last22=Baxter | first22=A. | last23=Belle | first23=J. | last24=Beltrame | first24=P. | last25=Bensinger | first25=J. | last26=Benson | first26=T. | last27=Bernard | first27=E.P. | last28=Bernstein | first28=A. | last29=Bhatti | first29=A. | last30=Biekert | first30=A. | journal=Nuclear Instruments and Methods in Physics Research Section A: Accelerators, Spectrometers, Detectors and Associated Equipment | volume=953 | page=163047 | s2cid=204800748 | display-authors=1 }}</ref><ref>{{Cite arXiv|title = LUX-ZEPLIN (LZ) Technical Design Report| eprint=1703.09144 | last1=Mount | first1=B. J. | last2=Hans | first2=S. | last3=Rosero | first3=R. | last4=Yeh | first4=M. | last5=Chan | first5=C. | last6=Gaitskell | first6=R. J. | last7=Huang | first7=D. Q. | last8=Makkinje | first8=J. | last9=Malling | first9=D. C. | last10=Pangilinan | first10=M. | last11=Rhyne | first11=C. A. | last12=Taylor | first12=W. C. | last13=Verbus | first13=J. R. | last14=Kim | first14=Y. D. | last15=Lee | first15=H. S. | last16=Lee | first16=J. | last17=Leonard | first17=D. S. | last18=Li | first18=J. | last19=Belle | first19=J. | last20=Cottle | first20=A. | last21=Lippincott | first21=W. H. | last22=Markley | first22=D. J. | last23=Martin | first23=T. J. | last24=Sarychev | first24=M. | last25=Tope | first25=T. E. | last26=Utes | first26=M. | last27=Wang | first27=R. | last28=Young | first28=I. | last29=Araújo | first29=H. M. | last30=Bailey | first30=A. J. | year=2017 | class=physics.ins-det | display-authors=1 }}</ref> This detector is the target for WIMP-nucleus scatters. As discussed in the next section, this detector can perform a 3-D reconstruction of the position of an interaction in the xenon. This enables an identification and rejection of background interactions that happen near the periphery (sides, top, and bottom) of the detector. These peripheral interactions are overwhelmingly likely to be from external gamma rays or neutrons and radioactive decays of trace radionuclides in the detector components composing the TPC and [[Physics:Cryostat|cryostats]]. Moreover, the relatively large density of liquid xenon allows the TPC to "self-shield" to a degree: gamma rays (neutrons) entering the TPC can travel only approximately a few centimeters (10 centimeters) before scattering and being stopped. As a result, the innermost volume of the detector is largely free of many of these backgrounds. Because it is so quiet, this innermost, or "fiducial" volume is very sensitive to observing WIMP scatters above other backgrounds, and is the space in which LZ's WIMP searches are conducted.

Next, the TPC is located inside several layers of active and passive shielding to reduce rates of external gamma rays and neutrons. The TPC is housed in an inner cryostat, which maintains the temperatures needed to keep the xenon in the liquid phase (approximately 178K). This inner cryostat is nested in a larger, outer cryostat, which helps limit heat transfer into the xenon. External to the outer cryostat is a set of acrylic tanks holding [[Physics:Scintillator|liquid scintillator]]. This scintillator is liquid-alkyl-benzene (LAB) loaded with [[Chemistry:Gadolinium|gadolinium]] for more efficient neutron capture. If a gamma ray or neutron scatters once inside the TPC but then exits, it will likely also deposit energy in the scintillator. These energy deposits are accompanied by emission of optical [[Physics:Photon|photons]], which can be detected by an array of [[Physics:Photomultiplier tube|photomultiplier tubes (PMTs)]] located outside of the acrylic tanks. By observing such a signal in coincidence with a scatter in the TPC, it becomes possible to reject backgrounds in the TPC that might otherwise look like WIMP scatters. This is particularly important for neutrons, which can penetrate farther than gamma rays and which scatter on the xenon nucleus in the same way that WIMPs are expected to (instead of on xenon's atomic electrons). The outer-detector PMT array is located in a larger water tank. Together, the water tank and liquid scintillator also provide significant passive shielding against external gamma rays and neutrons, stopping a vast majority of them before they have the chance to enter the TPC. The whole assembly is located approximately one mile underground, in the Davis Cavern at SURF. This underground location creates a rock overburden that significantly reduces the rate of cosmic ray muons entering the TPC relative to the rate at Earth's surface. All together these different strategies ensure that LZ is a detector capable of performing a very sensitive search for dark matter scatters on xenon nuclei.

== LZ's Inner Detector: Dual Phase TPC ==
[[File:DualPhaseTPCOperation.png|right|600x600px|A simple diagram of the operational principle of a dual-phase xenon TPC. During an interaction, S1 light (green) and S2 light (blue) are produced, and a fraction of each may be seen by the PMT arrays at the top and bottom of the detector. Note that this diagram is not to scale, and that LZ has many more than 4 PMTs in each array.]]
The detector at the heart of LZ is a cylindrical dual-phase xenon time projection chamber (TPC).<ref>{{Cite journal|title = The LUX-ZEPLIN (LZ) experiment| year=2020 | doi=10.1016/j.nima.2019.163047 | arxiv=1910.09124 | last1=Akerib | first1=D.S. | last2=Akerlof | first2=C.W. | last3=Akimov | first3=D.Yu. | last4=Alquahtani | first4=A. | last5=Alsum | first5=S.K. | last6=Anderson | first6=T.J. | last7=Angelides | first7=N. | last8=Araújo | first8=H.M. | last9=Arbuckle | first9=A. | last10=Armstrong | first10=J.E. | last11=Arthurs | first11=M. | last12=Auyeung | first12=H. | last13=Bai | first13=X. | last14=Bailey | first14=A.J. | last15=Balajthy | first15=J. | last16=Balashov | first16=S. | last17=Bang | first17=J. | last18=Barry | first18=M.J. | last19=Barthel | first19=J. | last20=Bauer | first20=D. | last21=Bauer | first21=P. | last22=Baxter | first22=A. | last23=Belle | first23=J. | last24=Beltrame | first24=P. | last25=Bensinger | first25=J. | last26=Benson | first26=T. | last27=Bernard | first27=E.P. | last28=Bernstein | first28=A. | last29=Bhatti | first29=A. | last30=Biekert | first30=A. | journal=Nuclear Instruments and Methods in Physics Research Section A: Accelerators, Spectrometers, Detectors and Associated Equipment | volume=953 | page=163047 | s2cid=204800748 | display-authors=1 }}</ref> This is composed of a 7 tonne liquid xenon target and a small region of gaseous xenon above. The operational principle is as follows. When a WIMP or background scatter occurs, a small amount of [[Physics:Kinetic energy|kinetic energy]] is given to a xenon nucleus (or atomic electron). This causes the xenon atom to ricochet around the area near the site of the scatter, converting its energy into the production of prompt [[Physics:Scintillation|scintillation]] photons, freed (ionization) electrons, and heat. A number of the prompt scintillation photons can be detected by the photomultiplier tubes (PMTs) at the top and bottom of the detector. The ionization electrons drift upward in an externally applied [[Physics:Electric field|electric field]], and upon reaching the liquid surface, are pulled into the gas and create [[Physics:Electroluminescence|electroluminescence]] light in a stronger electric field. This electroluminescence creates a delayed "S2" signal. The externally-created electric fields are created by a set of four [[Physics:High voltage|high voltage]] electrode grids: the bottom, the cathode, the gate, and the anode.<ref>{{Cite journal |last1=Linehan |first1=R. |last2=Mannino |first2=R. L. |last3=Fan |first3=A. |last4=Ignarra |first4=C. M. |last5=Luitz |first5=S. |last6=Skarpaas |first6=K. |last7=Shutt |first7=T. A. |last8=Akerib |first8=D. S. |last9=Alsum |first9=S. K. |last10=Anderson |first10=T. J. |last11=Araújo |first11=H. M. |date=2022-05-11 |title=Design and production of the high voltage electrode grids and electron extraction region for the LZ dual-phase xenon time projection chamber |url=https://www.sciencedirect.com/science/article/pii/S0168900221009062 |journal=Nuclear Instruments and Methods in Physics Research Section A: Accelerators, Spectrometers, Detectors and Associated Equipment |language=en |volume=1031 |pages=165955 |doi=10.1016/j.nima.2021.165955 |arxiv=2106.06622 |s2cid=235422518 |issn=0168-9002}}</ref> 

Taken together, the S1 and S2 enable precise 3D reconstruction of the position of an interaction in the xenon. Because the S2 happens very close to the upper PMT array, it alone can give a good sense of where in XY (i.e. relative to the detector axis) the interaction has occurred. The time difference between the prompt S1 and delayed S2 is a proxy for the depth of the interaction: by using the drift velocity of electrons in xenon at a given electric field, one can convert the drift time to a physical depth, or Z position. Together, this XYZ position permits one to identify a quiet inner fiducial volume for sensitive WIMP searches. It also enables discrimination between WIMP-like single-site interactions and background-like multi-site interactions, like those from neutrons or gamma rays.

Note that unlike other kinds of time projection chambers, such as those used in neutrino experiments like [[Physics:MicroBooNE|MicroBooNE]], the ionization signal here is fully captured via the S2 light - no current is directly measured by electrodes.

== LZ's WIMP Searches ==
[[File:WIMPsLZexperiment2023.png|thumb|Upper limits for WIMP-nucleon elastic cross sections from selected experiments as reported by the LZ experiment in July 2023.]]

In July 2022, the LZ collaboration published in a preprint its first upper limit on the spin-independent WIMP-nucleon scattering cross section, using approximately 60 livedays worth of data.<ref>{{Cite web|url=https://www.sciencenews.org/article/dark-matter-lz-experiment-physics|title = A supersensitive dark matter search found no signs of the substance — yet}}</ref><ref>{{Cite web |title=World's most sensitive dark matter detector starts collecting data {{!}} Imperial News {{!}} Imperial College London |url=https://www.imperial.ac.uk/news/238071/worlds-most-sensitive-dark-matter-detector/ |access-date=2022-07-07 |website=Imperial News |language=en}}</ref> Future searches intend to further probe for WIMP scatters, with a nominal search period of 1000 days.

On 28 July 2023 the LZ experiment first results of its searches for WIMPs previously released as a preprint were published on [[Physics:Physical Review Letters|Physics Review Letters]],<ref>{{Cite journal |last=Day |first=Charles |date=2023-07-28 |title=The Search for WIMPs Continues |url=https://physics.aps.org/articles/v16/s106 |journal=Physics |language=en |volume=16 |pages=s106 |doi=10.1103/PhysRevLett.131.041002|arxiv=2207.03764 }}</ref> excluding cross sections above <math>9.2\times10^{-48} cm^2</math> at 36 GeV with 90% confidence level,<ref>{{Cite journal |last=LUX-ZEPLIN Collaboration |last2=Aalbers |first2=J. |last3=Akerib |first3=D. S. |last4=Akerlof |first4=C. W. |last5=Al Musalhi |first5=A. K. |last6=Alder |first6=F. |last7=Alqahtani |first7=A. |last8=Alsum |first8=S. K. |last9=Amarasinghe |first9=C. S. |last10=Ames |first10=A. |last11=Anderson |first11=T. J. |last12=Angelides |first12=N. |last13=Araújo |first13=H. M. |last14=Armstrong |first14=J. E. |last15=Arthurs |first15=M. |date=2023-07-28 |title=First Dark Matter Search Results from the LUX-ZEPLIN (LZ) Experiment |url=https://link.aps.org/doi/10.1103/PhysRevLett.131.041002 |journal=Physical Review Letters |volume=131 |issue=4 |pages=041002 |doi=10.1103/PhysRevLett.131.041002|arxiv=2207.03764 }}</ref> jointly on the same date [[Physics:XENON#XENONnT|XENONnT]] published its first results too excluding cross sections above <math>2.58\times10^{-47} cm^2</math> at 28 GeV with 90% confidence level<ref>{{Cite journal |last=XENON Collaboration |last2=Aprile |first2=E. |last3=Abe |first3=K. |last4=Agostini |first4=F. |last5=Ahmed Maouloud |first5=S. |last6=Althueser |first6=L. |last7=Andrieu |first7=B. |last8=Angelino |first8=E. |last9=Angevaare |first9=J. R. |last10=Antochi |first10=V. C. |last11=Antón Martin |first11=D. |last12=Arneodo |first12=F. |last13=Baudis |first13=L. |last14=Baxter |first14=A. L. |last15=Bazyk |first15=M. |date=2023-07-28 |title=First Dark Matter Search with Nuclear Recoils from the XENONnT Experiment |url=https://link.aps.org/doi/10.1103/PhysRevLett.131.041003 |journal=Physical Review Letters |volume=131 |issue=4 |pages=041003 |doi=10.1103/PhysRevLett.131.041003|arxiv=2303.14729 }}</ref>

==References==
{{Reflist|}}

==External links==
*[http://lz.lbl.gov/ The LZ Dark Matter Experiment]
{{Dark matter}}

[[Category:Experiments for dark matter search]]
[[Category:Underground laboratories]]

{{Sourceattribution|LZ experiment}}