Historical plots

We display below some plots or figures that marked the history of neutrino physics. First list contains breakthrough and primary results. Second list contains summary plots which are milestones in neutrino knowledge. Those lists are non-exhaustive and are the arbitrary choice of the authors. It can evolve according to your suggestions.

Breakthrough and first results plots

1914

First result: Continuous beta spectrum measurement
[Cha14]

First beta spectrum measured by James Chadwick in 1914, while he was working in Germany. The figure shows the energy spectrum of the decay of Ra B+C: four spectral lines, identical to some previously found and a larger continuous spectrum.

1927

First result: Continuous beta spectrum measurement
[Ell27]

Beta spectrum measured by Ellis and Wooster. It figures out the number of electrons emitted by a radium beta-radioactive source, as a function of their energy. The curve is an extrapolation from the measurement points.

The continuous shape of the spectrum, unexpected for a two-body decay, triggered Wolfgang Pauli to “invent” the neutrino in his letter of December 1930.

1951

Scheme of the first neutrino project of F. Reines and C. Cowan
[Los97]

The idea was to detect the neutrinos produced by a nuclear explosion, with an underground detector close to the explosion area. Fortunately this “crazy” idea has not been used. This would have been a dark stain on the history of the neutrino.

1956

First result: Evidence for the neutrino by F. Reines and C. Cowan
[Rei53,Cow56,Rei56]

Fred Reines and Clyde Cowan performed a first experiment in 1953, close to the Hanford nuclear power plant [Rei53]. This was the Poltergeist project, whose detector is shown by the photograph. The result was not really significant. They improved their apparatus (bigger detector and better shielding against cosmic rays) and did a second experiment in 1956 at the Savannah River nuclear power plant. That led to the unambiguous evidence of neutrinos interactions in their detector [Cow56,Rei56].

[The generic term “neutrino” is used, but, to be exact, nuclear reactors emit anti-electron-neutrinos νe].

1958

First result: The Goldhaber experiment shows that neutrinos are left-handed
[Gol58]

The helicity of the neutrino is measured by a combined analysis of circular polarization and resonant scattering of gamma-rays following orbital electron capture.

Upper figure shows the scheme of the experiment: the source of 152mEu (0), at the top of the magnet (alternatively magnetized up and down), decays to an excited state of 152Sm with emission of 840 keV neutrinos, followed by a 960 keV gamma-ray. The gamma-rays which pass through the magnet are resonant-scattered from a Sm2O3 scatterer and detected by a NaI scintillator counter.

Lower figure shows the energy of the resonant-scattered gamma-rays. It contains both gamma-rays emitted from the 960 keV state (960 and 840 keV). It is deduced that the gamma-rays are circularly polarized and that their helicity is negative.

[See details in the original paper [Gol58]]

1962

First result: Observation of the muon-neutrinos νμ, a second family of neutrinos.
[Sch60,Pon59b,Dan62]

The idea that there could be a second family of neutrinos was proposed independently by Bruno Pontecorvo [Pon59b] and Melvin Schwartz [Sch60]. To observe this new family, Schwartz proposed the scheme shown in the upper figure. Difficult to imagine a more simple scheme which led to a great discovery and a Nobel prize!

This elegant scheme is at the origin of the spark chamber experiment  set up by Schwartz, Lederman and Steinberger at the Brookhaven laboratory in 1962 (see the photograph). Neutrinos come from the decay of pions produced in the proton interactions. About 100 muon-neutrino νμ interactions were observed [Dan62].

1965-1970

First neutrino interactions in bubble chambers [Pat65,Arg70]

The first neutrino interactions in (heavy liquid) bubble chambers were observed at CERN in 1964-1965 [Pat65] (no picture presently available).

The photograph shows the first neutrino-proton interaction observed on November 13th 1970 in the 12-ft hydrogen bubble chamber of the Argonne National Laboratory [Arg70].

Neutrino-nucleon cross section measurement

1972

First result: Measurement of neutrino-nucleon cross-section
[Per72]

Experimental measurements of the cross section (probability of interaction) of νμ on neutrons within nucleus of deuterium atoms. First figure shows that there is no significant increase of the cross-section with energy and confirms the very low value predicted by theory [reference still to be found].

The paper [Per72] gives also several cross sections of neutrino νμ and antineutrino νμ interactions. Second figures shows the elastic neutrino crosssections for various A mass hypothesis. Last figure displays the neutrino cross section on nucleon, showing the expected linear rising as a function of energy.

 

1973

First result: Discovery of Neutral Current interactions in the Gargamelle experiment
[Has73a] [Has73b]

This photograph shows the electron coming from the elastic interaction of a muon-antineutrino νμ with an electron in the Gargamelle bubble chamber, at CERN [Has73a]. This is the first evidence for leptonic neutral current (NC) interaction.

The discovery of the hadronic neutral current is shown on the lower figure [Has73b], where can be seen the number of NC (neutral current) and CC (charged current) events detected and their ratio with respect to their position in the bubble chamber, for neutrinos and anti-neutrinos.

In addition to the neutral current discovery, later measurements by Gargamelle and next experiments confirmed with great precision that NC/CC for neutrinos is xxx while NC/CC for anti-neutrinos is yyy

1968-1976

First result: Homestake solar neutrino experiment and the solar neutrino problem.
[Dav68,Bah76]

The radiochemical solar neutrino chlorine experiment was installed by Ray Davis in the Homestake mine in the middle of the 60’s. The principle was the transformation of 37Cl atoms induced by neutrinos νe into radioactive 37Ar atoms. The first results were published in 1968 [Dav68]. They showed for the first time the deficit of observed solar neutrino interactions compared to the predictions of solar models by John Bahcall. In the following years the updated results confirmed the deficit, giving rise to the so-called solar neutrino problem.
From 1976, the results were presented in the form of the well-known “Davis plot” (see figure), which showed the experimental measurements compared to the theoretical predictions.

1987

First results: Detection of neutrinos from SN1987A by Kamiokande and IMB
[Hir87] [Bio87]

The supernova SN1987A has been discovered in the Large Magellanic Cloud by Shelton in Chile (IAU Circular 4316, on February 24, 1987). Immediately, the physicists of the Kamiokande and IMB (Irvine-Michigan-Brookhaven) experiments analyzed their data and identified an excess of events, about 10 events in each experiment in about 10 seconds, on Feb 23, 1987, 07:35:41 UTC. These bursts of neutrino events, in coincidence with the SN1987A optical observation, mark the start of the neutrino astronomy.
The figure shows the time sequence of events observed in Kamiokande.

1989

First result : LEP finds 3 neutrino families
[Aar89,Ade90,Akr89,Dec89]

In a seminar at CERN on 13 october 1989, the four LEP experiments (ALEPH, DELPHI, L3 and OPAL) presented the first results on the Z line shapes. This measurement of the Z width provides information about the number of neutrino families. The data points shown here are the average hadronic cross-sections. The different curves on Alpeh and L3 plots correspond to the prediction for 2, 3 or 4 light neutrino species (the cross section decreases when the number of neutrino species increases). Three neutrino species is strongly favoured.

Neutrino oscillation seen by SuperK in 1998

to be added: Figure 2004 from Ash04

1998

First result: First observation of neutrino oscillation from atmospheric neutrinos in the SuperKamiokande experiment.
[Fuk98b,Kaj98,Ash04]

The first observation of oscillation of atmospheric neutrinos was made by the SuperKamiokande experiment in 1998 [Fuk98a,Kaj98]. The upper figure represents the angular distribution of νe events (left column) and νμ events (right column). Upper (lower) figures are for low (high) energy events. The deficit, compared to predictions, of  νμ events coming from the antipodes (cos(θ)<0) is the signature that they have been transformed into another flavor during their path.

In 2004, using only the high distance/energy (L/E) resolution event, SuperKamiokande showed that the measured νμ survival probability has a dip corresponding to the first minimum of the theoretical survival probability near L/E=(500km/GeV).  This was the first evidence that the neutrino survival probability obeys the sinusoidal function predicted by neutrino oscillations.The lower figure [Ash04].shows this survival probability as a function of L/E.

SNO and other solar neutrino results

2001

First result: SNO solves the solar neutrino problem
[Ahm01,Ahm02]

Mettre d’abord la première figure de SNO en 2001 (figure 3 du papier Ahm01).

Using heavy water (D2O) as a target to measure solar neutrinos, the SNO experiment was able to measure all the neutrino flavours (νe,νμ,ντ). This gave the first indication of a non electron flavor component in the solar neutrino flux and enabled the first determination of the total flux of 8B neutrinos generated by the Sun [Ahm01]. The upper figure shows the flux of (νμ+ντ) 8B solar neutrinos versus the pure νe flux measured by SNO via the pure charged current reaction (CC). For the elastic reaction, the results of SNO and SuperKamiokande are combined; the diagonal band shows the total flux (νe+νμ+ντ) experimental and theoretical; the intercept of the diagonal band with the vertical νe flux gives the νμ+ντ flux.

This result was completed in 2002 by a direct measurement of neutral-current interactions [Ahm02] (and later with more precise measurements)]. SNO made then an unambiguous detection of the flavor change of  neutrinos emitted in the core of the Sun.

The lower figure summarizes in 2018 the ratios of measurements to solar model calculations for SNO and all other solar neutrino experiments(Homestake, GALLEX, SAGE, SuperKamiokande). The SNO NC (Neutral Current) measurement is close to “one” (all the neutrino flavors are detected). The values differ for the different experiments since they have different energy thresholds to detect solar neutrinos but the values show clearly that the neutrino flavor change is the favored solution to what is happening to the solar neutrinos.
Figure ref : proceedings of the Neutrino History Conference, 5-7 sept. 2018.

Kamland first result in 2002Neutrino oscillation seen by KamLAND

2002

Summary: KamLAND observes neutrino oscillation
from nuclear reactors [Egu03]

KamLAND sees very well the oscillation of neutrinos from nuclear reactors. Data show the ratio of  the number of neutrinos observed to the number of neutrino expected if there were no neutrino oscillation. KamLAND was located at about 200 km of nuclear reactors and all the experiments before KamLAND were too close to the nuclear reactor (few km) to see the oscillation. The dashed curve shows the theoretical oscillation with the best fitting parameters for the KamLAND measurement’s point. The green area corresponds to the uncertainty on those parameters. This result reinforces the hypothesis of the so-called LMA solution of the solar neutrino problem.

2004

First result: KamLAND sees full neutrino oscillation
[Ara05b]

Neutrino oscillation seen by KamLAND. The “Survival Probability” is computed from the number of electron anti-neutrinos produced by the nuclear reactor and detected by KamLAND. It depends on the ratio between the distance  KamLAND-nuclear reactor and the energy of the neutrinos. The measurement points shows clearly the oscillation phenomena and its dependence on L/E.

DayaBay, RENO and DOuble Chooz results

2011

First result: Evidence for neutrino oscillation in reactor experiments.
[Abe11b,An12,Ahn12]

From 2004, several neutrino detectors were built close to nuclear power plants to search for the third neutrino mixing angle θ13.

The figure summarizes the first results of the Double Chooz, Daya Bay and RENO experiments. For each  experiment, the data of the upper plot are the number of neutrinos detected as a function of their energy, while the lower plots show the ratio between the measurements and the theoretical expectation in the case of no neutrino oscillation (Double Chooz) or the ratio between the number of neutrinos detected in the far and near detectors (Daya Bay, RENO), the near detector being the reference where no neutrino oscillation has yet occured.

At the same time, the T2K experiment also found evidence for a positive θ13 angle from νe appearance in a νμ beam [Abe11a].

Planck CMB measurement

2013

First result: The cosmological Planck experiment strongly favours 3 neutrino families
[Ade13]

The Planck experiment  provided a very good estimate of the number of neutrino families from the study of the Cosmic Microwave Background (CMB). The Planck satellite has measured the temperature of the CMB in all the directions of the Universe and looked at the temperature fluctuations for various angular scales (the l parameter on the x axis of the figure on the left). The first peak around l=100 corresponds to large fluctuations linked to baryogenesis and is called the baryonic acoustic peak. The red curve is a fit to the data, of which one parameter is the number of neutrino families. The best fit gives 3 neutrino families with an uncertainty of about 0.2 [Ade13].

 

Summary plots

1998

Summary: Homestake radiochemical solar neutrino experiment [Cle98].

The pioneer chlorine solar neutrino experiment run in the Homestake mine for 30 years (1968-1998). The figure shows the final result: each point gives the daily rate of radioactive 37Ar atoms produced by solar neutrinos and extracted from the 600 tons of the C2Cl4 solution of the detector. In SNU’s (solar neutrino units), the result is 2.56+-0.16+-0.16 about three times lower than the predictions of solar models (about 8 SNUs).

Gallex and Sage solar neutrino results

1992-1998

Summary:  Detection of pp solar neutrinos with radiochemical gallium experiments (GALLEX and SAGE) [Ans92,Abd94]

The chlorine solar neutrino experiment was not sensitive to the neutrinos coming from the primordial pp fusion reaction in the core of the Sun (which is directly linked to the luminosity of the Sun). In the middle of the 80’s, two experiments used gallium targets (lower threshold than the chlorine) to trap solar neutrinos by the transformation of 71Ga atoms into radioactive 71Ge atoms: GALLEX in the Gran Sasso underground laboratory and SAGE in the Baksan laboratory. The first GALLEX results, in 1992, (and later SAGE) confirmed the solar neutrino problem, with a deficit smaller than for the chlorine experiment.

The figure summarizes the experimental situation in 1998. The two experiments observe about 60% of the predictions of the solar models. The rate is measured  in SNU’s (Solar Neutrino Unit) [one SNU corresponds to 10−36 capture per target atom per second].

LEP measurements of the Z width

2000

Summary: LEP finds 3 families of light neutrinos
[Blo18]

In 1989, the first LEP measurements of the Z width provided information about the number of families of light neutrinos. The result has been improved in the following years and is shown in the left figure. The data points show theaverage hadronic cross-sections. The colored curves are the theoretical predictions depending on the number of neutrinos types which are active in the weak interaction. The curve with 3 neutrino types best fits the measurements. As mentioned on the plot, the errors bars have been increased by factor 10 to make them visible.

The figure corresponds to the data in 2000. The history is summarized in [Blo18].

2013

Summary: neutrino-nucleon total cross-section measurements
[Scu13]

The Ph.D. thesis by Scully in 2013 [Scu13] gives a brief review of the present knowledge of the neutrino and antineutrino cross sections. The figure on the left shows the total νμ CC (full line) and NC (dotted line) cross sections on deuterium as a function of the neutrino energy, compared with data on νμ CC from a variety of targets. The plot shows the linear increase of the cross-section with energy.

More information on neutrino cross-sections are found in [Scu13].

References

 Author(s)TitleReference
Aar89P. Aarnio et al., DELPHI Collaboration Measurement of the mass and the width of the Z particle from multi-hadronic final states produced in e+e- annihilations Phys. Lett. 231 (1989) 539
Abd94J.N. Abdurashitov et al. Results from SAGE (The Russian-American Gallium solar neutrino experiment)Phys. Lett. B328 (1994) 234
Abe11aK. Abe et al., T2K collaboration Indication of electron neutrino appearance from an accelerator-produced off-axis muon-neutrino beam Phys. Rev. Lett. 107 (2011) 041801; arXiv:1106.2822
Abe11bY. Abe et al., Double Chooz collaborationIndication for the disappearance of reactor electron antineutrinos in the Double Chooz experiment Phys. Rev. Lett. 108 (2012) 131801; arXiv:1112.6353
Ade13P.A.R. Ade et al. Planck 2013 Results. XVI. Cosmological Parameters Astronomy and Astrophysics 571 (2014) A16; arXiv:1303.5076
Ahm01Q.R. Ahmad et al., SNO collaboration Measurement of the rate ne + d → p + p + e- interactions produced by 8B solar neutrinos at the Sudbury Neutrino Observatory Phys. Rev. Lett. 87 (2001) 071301; arXiv:nucl-ex/0106015
Ahm02Q.R. Ahmad et al., SNO collaboration Direct evidence for neutrino flavor transformation from neutral-current interactions in the Sudbury Neutrino Observatory Phys. Rev. Lett. 89 (2002) 011301; arXiv:nucl-ex/0204008
Ahn12J.K. Ahn et al., RENO Collaboration Observation of reactor electron antineutrino disappearance in the RENO experimentPhys. Rev. Lett. 108 (2012) 191802; arXiv:1204.0626
Akr89M.Z. Akrawy et al., OPAL Collaboration Measurement of the Z mass and width the OPAL detector at LEPPhys. Lett. 231 (1989) 530
An12F.P. An et al., Daya Bay collaborationObservation of electron-antineutrino disappearance at Daya BayPhys. Rev. Lett. 108 (2012) 171803; arXiv:1203.1669
Ans92P. Anselmann et al., Gallex collaborationSolar neutrinos observed by GALLEX at Gran SassoPhys. Lett. B285 (1992) 376
Ara05bT. Araki et al., KamLAND collaborationMeasurement of neutrino oscillation with KamLAND: evidence of spectral distortionPhys. Rev. Lett. 94 (2005) 081801
Arg70Argonne LaboratoryThe neutrino event;
Ash04Y. Ashie et al., Super-Kamiokande collaboration Evidence for an oscillatory signature in atmospheric neutrino oscillationsPhys. Rev. Lett. 93 (2004) 101801
Bah76J.N. Bahcall and R. Davis Solar Neutrinos: A Scientific Puzzle Science 191 (1976) 264
Bio87R.M. Bionta et al., IMB collaborationObservation of a neutrino burst in coincidence with supernova SN1987A in the Large Magellanic Cloud Phys. Rev. Lett. 58 (1987) 1494
Blo18A. BlondelThe third family of neutrinosarXiv:1812.11362; Proceedings of the conference "History of the neutrino", 2019
Blo64M.M. Block et al. Neutrino interactions in the CERN heavy liquid bubble chamber Phys. Lett. 12 (1964) 281
Cha14J. Chadwick Intensitatsverteilung im magnetischen spektrum der beta-strahlen von radium B+CVerhandlungen der deutschen Physikalischen Gesellschaft 16 (1914) 383
Cle98B.T. Cleveland et al. Measurement of the solar electron neutrino flux with the Homestake chlorine detectorAstrophysical Journal 496 (1998) 505
Cow56C.L. Cowan, F. Reines, F.B. Harrison, H.W. Cruse and A.D. McGuire Detection of the free neutrino: a confirmationScience 124 (1956) 103, July 20, 1956
Dan62G. Danby, J.M. Gaillard, K. Goulianos, L.M. Lederman, N. Mistry, M. Schwartz and J. SteinbergerObservation of high energy neutrino reactions and the existence of two kinds of neutrinos Phys. Rev. Lett. 9 (1962) 36
Dav68R. Davis, D.S. Harmer, K.C. Hoffman Search for neutrinos from the Sun Phys. Rev. Lett. 20 (1968) 1205
Dec89D. Decamp et al., ALEPH Collaboration Determination of the number of light neutrino speciesPhys. Lett. 231 (1989) 519
Egu03K. Eguchi et al. First results from KamLAND: Evidence for reactor antineutrino disappearancePhys. Rev. Lett. 90 (2003) 021802
Ell27C.D. Ellis and W.A. Wooster The Average Energy of Disintegration of Radium E Proc. Roy. Soc. A 117 (1927) 109
Fuk98bY. Fukuda et al., Super-Kamiokande collaboration Evidence for oscillation of atmospheric neutrinos Phys. Rev. Lett. 81 (1998) 1562
Gol58M. Goldhaber, L. Grodzins, A. Sunyar Helicity of neutrinos Phys. Rev. 109 (1958) 1015
Has73aF.J. Hasert et al. Search for elastic muon-neutrino electron scattering Phys. Lett. B46 (1973) 121 – Received Jul. 2, 1973
Has73bF.J. Hasert et al. Observation of neutrino-like interactions without muon or electron in the Gargamelle neutrino experiment Phys. Lett. B46 (1973) 138 – Received July 23, 1973
Hir87K.S. Hirata et al., Kamiokande collaboration Observation of a neutrino burst from the supernova SN1987A Phys. Rev. Lett. 58 (1987) 1490
Kaj98Takaaki KajitaAtmospheric neutrino results from Super-Kamiokande and Kamiokande - Evidence for muon-neutrino oscillationsNucl. Phys. B (Proc. Suppl.) 77 (1999) 123
Los97Los AlamosCelebrating the neutrinoLos Alamos Science 25
Pat65Michel Paty Etudes d’interactions de neutrinos de grande énergie dans une chambre à bulles à liquide lourdCERN 65-12, 1965
Per72D. H. PerkinsNeutrino interactionsProc. of the 16th Int. Conf. On High-Energy Physics, Batavia (1972), vol. 4, p.189
Pon59bB. Pontecorvo Electron and muon neutrinos Soviet Physics JETP 10 (1960) 1236 ; J. Exp. Theoret. Phys. 37 (1959) 1751
Rei53F. Reines and C.L. Cowan Detection of the free neutrino Phys. Rev. 92 (1953) 830
Rei56Frederick Reines and Clyde Cowan jr.The neutrinoNature 178 (1956) 446
Sch60M. Schwartz Feasibility of using high energy neutrinos to study the weak interactionsPhys. Rev. Lett. 4 (1960) 306
Scu13Daniel Ivan ScullyNeutrino induced coherent pion productionPh. D. thesis, Univ. of Warwick (2013)

 

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