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The K2K experiment (KEK to Kamioka) was a neutrino experiment that ran from June 1999 to November 2004. It used muon neutrinos from a well-controlled and well-understood beam to verify the oscillations previously observed by Super-Kamiokande using atmospheric neutrinos. This was the first positive measurement of neutrino oscillations in which both the source and detector were fully under experimenters' control.^[1]^[2] Previous experiments relied on neutrinos from the Sun or from cosmic sources. The experiment found oscillation parameters which were consistent with those measured by Super-Kamiokande.

Experimental design

K2K is a neutrino experiment which directed a beam of muon neutrinos (
ν
_μ) from the 12 GeV proton synchrotron at the KEK, located in Tsukuba, Ibaraki, to the Kamioka Observatory, located in Kamioka, Gifu, about 250 km away.^[3] The muon neutrinos travelled through Earth, which allowed them to oscillate (change) into other flavours of neutrinos, namely into electron neutrinos (
ν
_e) and tau neutrinos (
ν
_τ). K2K however, focused only on
ν
_μ →
ν
_τ oscillations.^[4]

The proton beam from the synchrotron was directed onto an aluminium target, and the resulting collisions produced a copious amount of pions. These pions were then focused into a 200 m decay pipe, where they would decay into muons and muon neutrinos.^[3] The muons were stopped at the end of the pipe, leaving a beam of muon neutrinos. The exact composition of the beam contained over 97% muon neutrinos, with the other 3% being made of electron neutrinos (
ν
_e), electron antineutrinos (
ν
_e) and muon antineutrinos (
ν
_μ).^[4]

After they exited the pipe, the neutrinos went through a 1-kiloton water Cherenkov neutrino detector ("near detector") located at about 300 m from the aluminium target to determine the neutrino beam characteristics. This 1-kiloton "near detector" was a scaled-down version of the 50-kiloton Super-Kamiokande "far detector" located at the Kamioka Observatory, which allowed scientists to eliminate certain systematic uncertainties that would be present if two different detector types were used.^[5] This dual-detector configuration allowed the comparison of the neutrino beam at the near detector with the neutrino beam at the far detector to determine if neutrinos had oscillated or not.^[6]

Collaboration

The K2K collaboration consisted of roughly 130 physicists from 27 universities and research institutes from all over the world, listed below.^[7] The full list of scientists and their countries of origin is available on the K2K website.

Results

The final K2K results found that at 99.9985% confidence (4.3 σ) there had been a disappearance of muon neutrinos. Fitting the data under the oscillation hypothesis, the best fit for the square of the mass difference between muon neutrinos and tau neutrinos was Δm² = 2.8×10⁻³ eV².^[4] This result is in good agreement with the previous Super-Kamiokande result,^[8] and the later MINOS result.^[9]

References

^ "Synthetic neutrinos appear to disappear". CERN Courier. 40 (7). 18 August 2000.
^ N. Nosengo (2006). "Neutrinos make a splash in Italy". Nature. 443 (7108): 126. Bibcode:2006Natur.443..126N. doi:10.1038/443126a. PMID 16971911.
^ ^a ^b "Long Baseline neutrino oscillation experiment, from KEK to Kamioka (K2K)". High Energy Accelerator Research Organization. 13 June 2002. Retrieved 3 September 2010.
^ ^a ^b ^c M. H. Ahn; et al. (K2K Collaboration) (2006). "Measurement of Neutrino Oscillation by the K2K Experiment". Physical Review D. 74 (7): 072003. arXiv:hep-ex/0606032. Bibcode:2006PhRvD..74g2003A. doi:10.1103/PhysRevD.74.072003. S2CID 22053653.
^ "K2K: Near Detector". [Stony Brook Super-Kamiokande/K2K group]. 19 June 1999. Retrieved 3 September 2010.
^ "K2K: Introduction". [Stony Brook Super-Kamiokande/K2K group]. 20 June 1999. Retrieved 3 September 2010.
^ "K2K Member Institutes". High Energy Accelerator Research Organization. 20 January 2004. Retrieved 3 September 2010.
^ Y. Fukuda; et al. (Super-K Collaboration) (1998). "Measurements of the Solar Neutrino Flux from Super-Kamiokande's First 300 Days". Physical Review Letters. 81 (6): 1158–1162. arXiv:hep-ex/9805021. Bibcode:1998PhRvL..81.1158F. doi:10.1103/PhysRevLett.81.1158. S2CID 14217731. and erratum "Erratum: Measurements of the Solar Neutrino Flux from Super-Kamiokande's First 300 Days". Physical Review Letters. 81 (19): 4279. 1998. Bibcode:1998PhRvL..81.4279F. doi:10.1103/PhysRevLett.81.4279.
^ D.G. Michael; et al. (MINOS Collaboration) (2006). "Observation of muon neutrino disappearance with the MINOS detectors in the NuMI neutrino beam". Physical Review Letters. 97 (19): 191801. arXiv:hep-ex/0607088. Bibcode:2006PhRvL..97s1801M. doi:10.1103/PhysRevLett.97.191801. PMID 17155614. S2CID 119458915.

External links

[1] "Synthetic neutrinos appear to disappear". CERN Courier. 40 (7). 18 August 2000.

[2] N. Nosengo (2006). "Neutrinos make a splash in Italy". Nature. 443 (7108): 126. Bibcode:2006Natur.443..126N. doi:10.1038/443126a. PMID 16971911.

[K2K_intro-3] "Long Baseline neutrino oscillation experiment, from KEK to Kamioka (K2K)". High Energy Accelerator Research Organization. 13 June 2002. Retrieved 3 September 2010.

[K2K_results-4] M. H. Ahn; et al. (K2K Collaboration) (2006). "Measurement of Neutrino Oscillation by the K2K Experiment". Physical Review D. 74 (7): 072003. arXiv:hep-ex/0606032. Bibcode:2006PhRvD..74g2003A. doi:10.1103/PhysRevD.74.072003. S2CID 22053653.

[NEAR-5] "K2K: Near Detector". [Stony Brook Super-Kamiokande/K2K group]. 19 June 1999. Retrieved 3 September 2010.

[K2K_intro-2-6] "K2K: Introduction". [Stony Brook Super-Kamiokande/K2K group]. 20 June 1999. Retrieved 3 September 2010.

[7] "K2K Member Institutes". High Energy Accelerator Research Organization. 20 January 2004. Retrieved 3 September 2010.

[8] Y. Fukuda; et al. (Super-K Collaboration) (1998). "Measurements of the Solar Neutrino Flux from Super-Kamiokande's First 300 Days". Physical Review Letters. 81 (6): 1158–1162. arXiv:hep-ex/9805021. Bibcode:1998PhRvL..81.1158F. doi:10.1103/PhysRevLett.81.1158. S2CID 14217731. and erratum "Erratum: Measurements of the Solar Neutrino Flux from Super-Kamiokande's First 300 Days". Physical Review Letters. 81 (19): 4279. 1998. Bibcode:1998PhRvL..81.4279F. doi:10.1103/PhysRevLett.81.4279.

[9] D.G. Michael; et al. (MINOS Collaboration) (2006). "Observation of muon neutrino disappearance with the MINOS detectors in the NuMI neutrino beam". Physical Review Letters. 97 (19): 191801. arXiv:hep-ex/0607088. Bibcode:2006PhRvL..97s1801M. doi:10.1103/PhysRevLett.97.191801. PMID 17155614. S2CID 119458915.

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[2]

[3]

[4]

[5]

[6]

[7]

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[9]

@@ Line 1: / Line 1: @@
+{{Use dmy dates|date=May 2021}}
-The '''K2K experiment''' ([[KEK]] to [[Kamioka Observatory|Kamioka]]) was a [[List of neutrino experiments|neutrino experiment]] that ran from June 1999 to November 2004. It used [[muon neutrino]]s from a well-controlled and well-understood [[particle beam|beam]] to verify the [[neutrino oscillation|oscillations]] previously observed by  [[Super-Kamiokande]] using [[Neutrino#Atmospheric neutrinos|atmospheric neutrinos]]. This was the first positive measurement of [[neutrino oscillations]] in which both the source and detector were fully under experimenters' control.<ref>
+The '''K2K experiment''' ([[KEK]] to [[Kamioka Observatory|Kamioka]]) was a [[List of neutrino experiments|neutrino experiment]] that ran from June 1999 to November 2004. It used [[muon neutrino]]s from a well-controlled and well-understood [[Accelerator neutrino|beam]] to verify the [[neutrino oscillation|oscillations]] previously observed by [[Super-Kamiokande]] using [[Neutrino#Atmospheric neutrinos|atmospheric neutrinos]]. This was the first positive measurement of [[neutrino oscillations]] in which both the source and detector were fully under experimenters' control.<ref>
 {{cite journal
- |author=
  |date=18 August 2000
  |title=Synthetic neutrinos appear to disappear
@@ Line 10: / Line 10: @@
 {{cite journal
  |author=N. Nosengo
- |year=2006
+ |date=2006
  |title=Neutrinos make a splash in Italy
  |journal=[[Nature (journal)|Nature]]
@@ Line 16: / Line 16: @@
  |volume=443 |issue=7108 |pages=126
  |doi=10.1038/443126a
+|bibcode = 2006Natur.443..126N |url=https://cds.cern.ch/record/988253
-}}</ref> Previous experiments relied on neutrinos [[Neutrino#Solar neutrinos|from the Sun]] or from [[cosmic ray|cosmic sources]]. The experiment found oscillation parameters which were consistent with those measured by Super-Kamiokande.
+ |doi-access=free
+ }}</ref> Previous experiments relied on neutrinos [[Neutrino#Solar neutrinos|from the Sun]] or from [[cosmic ray|cosmic sources]]. The experiment found oscillation parameters which were consistent with those measured by Super-Kamiokande.
 ==Experimental design==
-[[Image:Super-k.jpg|thumb|The inside of the 50-kiloton [[Super-Kamiokande]] detector ("far detector").]]
+<!-- Deleted image removed: [[Image:Super-k.jpg|thumb|The inside of the 50-kiloton [[Super-Kamiokande]] detector ("far detector").]] -->
-K2K is a [[List of neutrino experiments|neutrino experiment]] which directed a beam of [[muon neutrino]]s ({{SubatomicParticle|muon neutrino}}) from the {{val|12|ul=GeV}} [[proton]] [[synchrotron]] at the [[KEK]], located in [[Tsukuba, Ibaraki|Tsukuba]], [[Ibaraki Prefecture|Ibaraki]], to the [[Kamioka Observatory]], located in [[Kamioka]], [[Gifu Prefecture|Gifu]], about 250&nbsp;km away.<ref name="K2K intro">
+K2K is a [[List of neutrino experiments|neutrino experiment]] which directed a [[Accelerator neutrino|beam]] of [[muon neutrino]]s ({{Subatomic particle|muon neutrino}}) from the {{val|12|ul=GeV}} [[proton]] [[synchrotron]] at the [[KEK]], located in [[Tsukuba, Ibaraki|Tsukuba]], [[Ibaraki Prefecture|Ibaraki]], to the [[Kamioka Observatory]], located in [[Kamioka]], [[Gifu Prefecture|Gifu]], about 250&nbsp;km away.<ref name="K2K intro">
 {{cite web
  |date=13 June 2002
@@ Line 27: / Line 29: @@
  |url=http://neutrino.kek.jp/intro/k2k.html
  |publisher=[[KEK|High Energy Accelerator Research Organization]]
- |accessdate=2010-09-03
+ |access-date=2010-09-03
-}}</ref> The muon neutrinos travelled through [[Earth]], which allowed them to [[neutrino oscillation|oscillate]] (change) into other [[flavour (particle physics)|flavours]] of [[neutrino]]s, namely into [[electron neutrino]]s ({{SubatomicParticle|electron neutrino}})  and [[tau neutrino]]s ({{SubatomicParticle|tau neutrino}}). K2K however, focused only on {{nowrap|{{SubatomicParticle|muon neutrino}} → {{SubatomicParticle|tau neutrino}}}} oscillations.<ref name="K2K results"/>
+}}</ref> The muon neutrinos travelled through [[Earth]], which allowed them to [[neutrino oscillation|oscillate]] (change) into other [[flavour (particle physics)|flavours]] of [[neutrino]]s, namely into [[electron neutrino]]s ({{Subatomic particle|electron neutrino}}) and [[tau neutrino]]s ({{Subatomic particle|tau neutrino}}). K2K however, focused only on {{nowrap|{{Subatomic particle|muon neutrino}} → {{Subatomic particle|tau neutrino}}}} oscillations.<ref name="K2K results"/>
-The proton beam from the synchrotron was directed onto an [[aluminium]] target, and the resulting collisions produced a copious amount of [[pion]]s. These pions were then focused into a 200&nbsp;m decay pipe, where they would [[particle decay|decay]] into [[muon]]s and [[muon neutrino]]s.<ref name="K2K intro"/>  The muons were stopped at the end of the pipe, leaving a beam of muon neutrinos. The exact composition of the beam contained over 97% muon neutrinos, with the other 3% being made of electron neutrinos ({{SubatomicParticle|electron neutrino}}), electron antineutrinos ({{SubatomicParticle|electron antineutrino}}) and muon antineutrinos ({{SubatomicParticle|muon antineutrino}}).<ref name="K2K results"/>
+The proton beam from the synchrotron was directed onto an [[aluminium]] target, and the resulting collisions produced a copious amount of [[pion]]s. These pions were then focused into a 200&nbsp;m decay pipe, where they would [[particle decay|decay]] into [[muon]]s and [[muon neutrino]]s.<ref name="K2K intro"/> The muons were stopped at the end of the pipe, leaving a beam of muon neutrinos. The exact composition of the beam contained over 97% muon neutrinos, with the other 3% being made of electron neutrinos ({{Subatomic particle|electron neutrino}}), electron antineutrinos ({{Subatomic particle|electron antineutrino}}) and muon antineutrinos ({{Subatomic particle|muon antineutrino}}).<ref name="K2K results"/>
-After they exited the pipe, the neutrinos went through a 1-kiloton [[water]] [[Cherenkov detector|Cherenkov]] [[neutrino detector]] ("near detector") located at about 300&nbsp;m from the aluminium target to determine the neutrino beam characteristics. This 1-kiloton "near detector" was a scaled-down version of the 50-kiloton [[Super-Kamiokande]] "far detector" located at the [[Kamioka Observatory]], which allowed scientists to eliminate certain systematic uncertainties that would be present if two different detector types were used.<ref name=NEAR>
+After they exited the pipe, the neutrinos went through a 1-kiloton [[water]] [[Cherenkov detector|Cherenkov]] [[neutrino detector]] ("near detector") located at about 300&nbsp;m from the aluminium target to determine the [[Accelerator neutrino|neutrino beam]] characteristics. This 1-kiloton "near detector" was a scaled-down version of the 50-kiloton [[Super-Kamiokande]] "far detector" located at the [[Kamioka Observatory]], which allowed scientists to eliminate certain systematic uncertainties that would be present if two different detector types were used.<ref name=NEAR>
 {{cite web
- |author=
  |date=19 June 1999
  |title=K2K: Near Detector
  |url=http://k2k.physics.sunysb.edu/k2k/near_detector.shtml
- |publisher=[http://nngroup.physics.sunysb.edu/nngroup/ Stony Brook Super-Kamiokande/K2K group]
+ |publisher=[Stony Brook Super-Kamiokande/K2K group]
- |accessdate=2010-09-03
+ |access-date=2010-09-03
 }}</ref> This dual-detector configuration allowed the comparison of the neutrino beam at the near detector with the neutrino beam at the far detector to determine if neutrinos had oscillated or not.<ref name="K2K intro-2">
 {{cite web
- |author=
  |date=20 June 1999
  |title=K2K: Introduction
  |url=http://k2k.physics.sunysb.edu/k2k/intro.shtml
- |publisher=[http://nngroup.physics.sunysb.edu/nngroup/ Stony Brook Super-Kamiokande/K2K group]
+ |publisher=[Stony Brook Super-Kamiokande/K2K group]
- |accessdate=2010-09-03
+ |access-date=2010-09-03
 }}</ref>
@@ Line 53: / Line 53: @@
 The K2K collaboration consisted of roughly 130 physicists from 27 universities and research institutes from all over the world, listed below.<ref>
 {{cite web
- |author=
  |date=20 January 2004
  |title=K2K Member Institutes
  |url=http://neutrino.kek.jp/member.html
  |publisher=[[KEK|High Energy Accelerator Research Organization]]
- |accessdate=2010-09-03
+ |access-date=2010-09-03
 }}</ref> The full list of scientists and their countries of origin is available on the [http://neutrino.kek.jp/member.html K2K website].
+{{div col|colwidth=22em}}
-{{columns-list|2|
 *[[Boston University]]
 *[[Chonnam National University]]
-*[[CEA Saclay|Commissariat à l'énergie atomique de Saclay]] (DSM-DAPNIA)
+*[[CEA Saclay]] (DSM-DAPNIA)
 *[[Dongshin University]]
 *[[KEK|High Energy Accelerator Research Organization]]
@@ Line 80: / Line 79: @@
 *[[Tokyo University of Science]]
 *[[Tohoku University]]
-*[[University of Barcelona]]
+*[[Autonomous University of Barcelona]]/[[IFAE]]
 *[[University of California, Irvine]]
 *[[University of Geneva]]
 *[[University of Hawaii]]
 *[[University of Tokyo]]
-*[[University of Washington]]
 *[[University of Valencia]]
 *[[University of Warsaw]]
+*[[University of Washington]]
-}}
+{{div col end}}
 ==Results==
-The final K2K results found that at 99.9985% confidence (4.3&nbsp;[[standard deviation|&sigma;]]) there had been a disappearance of muon neutrinos. Fitting the data under the oscillation hypothesis, the [[curve fitting|best fit]] for the square of the mass difference between muon neutrinos and tau neutrinos was (Δ''m'')<sup>2</sup>&nbsp;=&nbsp;{{val|2.8|e=-3|u=eV<sup>2</sup>}}.<ref name="K2K results">
+The final K2K results found that at 99.9985% confidence (4.3&nbsp;[[standard deviation|σ]]) there had been a disappearance of muon neutrinos. Fitting the data under the oscillation hypothesis, the [[curve fitting|best fit]] for the square of the mass difference between muon neutrinos and tau neutrinos was Δ''m''<sup>2</sup>&nbsp;=&nbsp;{{val|2.8|e=-3|u=eV<sup>2</sup>}}.<ref name="K2K results">
 {{cite journal
-|author = M. H. Ahn ''et al''. (K2K Collaboration)
+|author = M. H. Ahn
+|collaboration=[[K2K experiment#Collaboration|K2K Collaboration]]
 |year = 2006
 |title = Measurement of Neutrino Oscillation by the K2K Experiment
@@ Line 100: / Line 100: @@
 |volume = 74|pages = 072003
 |doi = 10.1103/PhysRevD.74.072003
-|id =
 |arxiv=hep-ex/0606032
+|bibcode = 2006PhRvD..74g2003A
+|issue = 7 |s2cid=22053653
 }}</ref> This result is in good agreement with the previous [[Super-Kamiokande]] result,<ref>
 {{cite journal
- |author=Y. Fukuda ''et al''. ([[Super-Kamiokande|Super-K Collaboration]])
+ |author=Y. Fukuda
+ |collaboration=[[Super-Kamiokande|Super-K Collaboration]]
- |year=1998
+ |date=1998
  |title=Measurements of the Solar Neutrino Flux from Super-Kamiokande's First 300 Days
  |journal=[[Physical Review Letters]]
- |volume=81 |pages=1158
+ |volume=81 |pages=1158–1162
  |doi=10.1103/PhysRevLett.81.1158
 |bibcode=1998PhRvL..81.1158F
+|arxiv = hep-ex/9805021
-}} and erratum {{cite journal
+ |issue=6 |s2cid=14217731
+ }} and erratum {{cite journal
  |author=<!--No need for them-->
- |year=1998
+ |date=1998
+ |title=Erratum: Measurements of the Solar Neutrino Flux from Super-Kamiokande's First 300 Days
- |title=<!--No need for it-->
  |journal=[[Physical Review Letters]]
  |volume=81 |pages=4279
  |doi=10.1103/PhysRevLett.81.4279
 |bibcode=1998PhRvL..81.4279F
+ |issue=19
-}}</ref> and the later [[MINOS]] result.<ref>
+|doi-access=free
+ }}</ref> and the later [[MINOS]] result.<ref>
 {{cite journal
- |author=D.G. Michael ''et al''. ([[MINOS|MINOS Collaboration]])
+ |author=D.G. Michael
+ |collaboration=[[MINOS|MINOS Collaboration]]
  |year=2006
  |title=Observation of muon neutrino disappearance with the MINOS detectors in the NuMI neutrino beam
@@ Line 127: / Line 134: @@
  |volume=97 |pages=191801
  |doi=10.1103/PhysRevLett.97.191801
- |id=
 |pmid=17155614
 |arxiv=hep-ex/0607088
 |bibcode=2006PhRvL..97s1801M
+ |issue=19
-}}</ref>
+|s2cid=119458915
+ }}</ref>
 ==See also==
@@ Line 137: / Line 145: @@
 ==References==
-{{Reflist|2}}
+{{reflist}}
 ==External links==
@@ Line 143: / Line 151: @@
 *[http://neutrino.kek.jp/publications/ K2K publications]
+{{Breakthrough Prize laureates}}
 {{neutrino detectors}}

v t e Breakthrough Prize laureates
Mathematics	Simon Donaldson, Maxim Kontsevich, Jacob Lurie, Terence Tao and Richard Taylor (2015) Ian Agol (2016) Jean Bourgain (2017) Christopher Hacon, James McKernan (2018) Vincent Lafforgue (2019) Alex Eskin (2020) Martin Hairer (2021) Takuro Mochizuki (2022) Daniel A. Spielman (2023) Simon Brendle (2024)
Fundamental physics	Nima Arkani-Hamed, Alan Guth, Alexei Kitaev, Maxim Kontsevich, Andrei Linde, Juan Maldacena, Nathan Seiberg, Ashoke Sen, Edward Witten (2012) Special: Stephen Hawking, Peter Jenni, Fabiola Gianotti (ATLAS), Michel Della Negra, Tejinder Virdee, Guido Tonelli, Joseph Incandela (CMS) and Lyn Evans (LHC) (2013) Alexander Polyakov (2013) Michael Green and John Henry Schwarz (2014) Saul Perlmutter and members of the Supernova Cosmology Project; Brian Schmidt, Adam Riess and members of the High-Z Supernova Team (2015) Special: Ronald Drever, Kip Thorne, Rainer Weiss and contributors to LIGO project (2016) Yifang Wang, Kam-Biu Luk and the Daya Bay team, Atsuto Suzuki and the KamLAND team, Kōichirō Nishikawa and the K2K / T2K team, Arthur B. McDonald and the Sudbury Neutrino Observatory team, Takaaki Kajita and Yōichirō Suzuki and the Super-Kamiokande team (2016) Joseph Polchinski, Andrew Strominger, Cumrun Vafa (2017) Charles L. Bennett, Gary Hinshaw, Norman Jarosik, Lyman Page Jr., David Spergel (2018) Special: Jocelyn Bell Burnell (2018) Charles Kane and Eugene Mele (2019) Special: Sergio Ferrara, Daniel Z. Freedman, Peter van Nieuwenhuizen (2019) The Event Horizon Telescope Collaboration (2020) Eric Adelberger, Jens H. Gundlach and Blayne Heckel (2021) Special: Steven Weinberg (2021) Hidetoshi Katori and Jun Ye (2022) Charles H. Bennett, Gilles Brassard, David Deutsch, Peter W. Shor (2023) John Cardy and Alexander Zamolodchikov (2024)
Life sciences	Cornelia Bargmann, David Botstein, Lewis C. Cantley, Hans Clevers, Titia de Lange, Napoleone Ferrara, Eric Lander, Charles Sawyers, Robert Weinberg, Shinya Yamanaka and Bert Vogelstein (2013) James P. Allison, Mahlon DeLong, Michael N. Hall, Robert S. Langer, Richard P. Lifton and Alexander Varshavsky (2014) Alim Louis Benabid, Charles David Allis, Victor Ambros, Gary Ruvkun, Jennifer Doudna and Emmanuelle Charpentier (2015) Edward Boyden, Karl Deisseroth, John Hardy, Helen Hobbs and Svante Pääbo (2016) Stephen J. Elledge, Harry F. Noller, Roeland Nusse, Yoshinori Ohsumi, Huda Zoghbi (2017) Joanne Chory, Peter Walter, Kazutoshi Mori, Kim Nasmyth, Don W. Cleveland (2018) C. Frank Bennett and Adrian R. Krainer, Angelika Amon, Xiaowei Zhuang, Zhijian Chen (2019) Jeffrey M. Friedman, Franz-Ulrich Hartl, Arthur L. Horwich, David Julius, Virginia Man-Yee Lee (2020) David Baker, Catherine Dulac, Dennis Lo, Richard J. Youle [de] (2021) Jeffery W. Kelly, Katalin Karikó, Drew Weissman, Shankar Balasubramanian, David Klenerman and Pascal Mayer (2022) Clifford P. Brangwynne, Anthony A. Hyman, Demis Hassabis, John Jumper, Emmanuel Mignot, Masashi Yanagisawa (2023) Carl June, Michel Sadelain, Sabine Hadida, Paul Negulescu, Fredrick Van Goor, Thomas Gasser, Ellen Sidransky and Andrew Singleton (2024)