UHECR by lightest nuclei in Nearby Universe and its parasite neutrino trace

UHECR by lightest nuclei in Nearby Universe and its parasite neutrino trace

Abstract

UHECR mystery survived first Auger claims of AGN connection within a GZK (100 Mpc size) Universe. Last 2010 UHECR maps and compositions do show a much lower correlation with AGN SuperGalactic maps and with protons (the two main ingredient of that claim). The three main AUGER results that survived are: an embarrassing absence of Virgo cluster UHECR, an expected signal; a steady presence of Cen-A clustering and a remarkable signature of nuclei (not nucleon) composition. We claim that the He-like lightest nuclei may solve most of the puzzle: He UHECR cannot arrive from Virgo because light nuclei fragility and opacity; Cen-A UHECR are spread (if He-Li-Be) as much as the observed ones; the light nuclei may fit well Auger composition signature as well as Hires spectra. Future multiplet of half energy UHECR must trace in tails some of UHECRa. Their secondaries GZK neutrinos will crowd not at thousand PeV, but more at tens PeV observable maybe in ICECUBE and also in horizontal tau airshowers in ARGO or by upward tau airshowers in Auger and TA fluorescence telescopes.

32nd International Cosmic Ray Conference, Beijing 2011 UHECR by lightest nuclei in Nearby Universe and its parasite neutrino trace
Daniele Fargion
Physics Department, Rome University 1, Sapienza, Ple.A.Moro 2, Rome,Italy
INFN Rome 1
daniele.fargion@Roma1.infn.it

Abstract:

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1 UHECR by He and the fragments

UHECR astronomy is becoming a reality, with some confusion because of the magnetic field smearing of their arrival directions. Moreover while flying UHECR are making photo-pion (if nucleon) or gamma and neutrinos by photo-dissociation (if light nuclei). Making UHECR nucleon local and sharp (GZK cut off, tens Mpc) or very local and smeared (a few Mpc) for lightest nuclei, or making UHECR astronomy meaningless if made by iron or other heavy nuclei. Therefore any UHECR astronomy is surrounded by a parasite astronomy made by gamma and neutrinos as well as by their possible small radio tails and UHECR fragments. Indeed UHECR formed by lightest nuclei may explain clustering of events around CenA and a puzzling UHECR absence around Virgo. Their fragments may trace on the same UHECR maps by a secondary tail or a crown clustering at half or fourth the UHECR primary energy. Neutrinos and gamma are tracing (both for nucleon or nuclei) their UHECR trajectory, respectively at EeVs or PeV energy. Gamma rays are partially absorbed by microwave and infrared background making only a very local limited astronomy. Among neutrinos , muons ones , the most penetrating and easy to detect, are deeply polluted by atmospheric component (smeared and isotropic like their parent CR ). As shown by last TeV muon neutrino maps probed by very smooth ICECUBE neutrinos map. Tau neutrinos, the last neutral lepton discovered, absent in neutrino oscillation at TeVs-PeVs-EeVs atmospheric windows, may arise as the first clean signal in UHECR-neutrino associated astronomy. Their tau birth in ice may shine as a double bangs (disentangled above PeV) anisotropy. In addition UHE tau, born tangent to the Earth or mountain, while escaping in air may lead, by decay in flight, to loud, amplified well detectable tau-airshower at horizons. Tau astronomy versus UHECR are going to reveal most violent sky as the most deepest probe. First hint of Vela, the brightest and nearest gamma source, a first galactic source is rising as a UHECR triplet nearby. Cen A (the most active and nearby AGN) is apparently shining UHECR source whose clustering (almost a quarter of the event) along a narrow solid angle around (whose opening angular size is ) seem firm and it is favoring lightest nuclei. Remaining events are possibly more smeared being more bent and heavier nuclei of galactic and-or extragalactic origin. The rise of nucleon UHECR above GZK astronomy made by protons (AUGER November 2007) is puzzled by three main mysteries: an unexpected nearby Virgo UHECR suppression (or absence), a rich crowded clustering frozen vertically along Cen A, a composition suggesting nuclei (not much directional) and not nucleons. The UHECR map, initially consistent with GZK volumes, to day seem to be not much correlated with expected Super Galactic Plane. Moreover slant depth data of UHECR from AUGER airshower shape do not favor the proton but points to a nuclei. To make even more confusion (or fun) HIRES, on the contrary, seem to favor, but with less statistical weight, UHECR mostly nucleons. We tried (at least partially) to solve the contradictions assuming UHECR as light nuclei ( , Li, Be)) spread by planar galactic fields, randomly at vertical axis. The fragility and its mass and its charge explains naturally the Virgo absence (due to opacity above few Mpc) and the observed wide Cen A spread clustering (a quarter of the whole sample within ). However more events and rarest doublets and clustering are waiting for an answer. Here we foresee hint of a new UHECR component, due to a first timid triplet toward Vela, the nearest and the brightest gamma source (at few or tens GeV) as well as the possible first high energy source (cosmic ray at tens TeV). Indeed early anisotropy of tens TeVs Cosmic rays found in ICECUBE muons might confirm this possibility. Let us remind that last century have seen the birth of a puzzling cosmic ray whose nature and origination has been and it is still growing in an apparent never-ending chain of puzzle. The Cosmic Black Body Radiation had imposed since a cut, GZK cut-off [15], of highest energy cosmic ray propagation, implying a very limited cosmic Volume (ten or few tens Mpc) for highest UHECR nucleon events. Because of the UHECR rigidity one had finally to expect to track easily UHECR directionality back toward the sources into a new Cosmic Rays Astronomy. Indeed in last two decades, namely since 1991-1995 the rise of an apparent UHECR at eV, by Fly’s Eye, has opened the wondering of its origination: no nearby (within GZK cut off) source have been correlated. Incidentally it should be noted that even after two decades and after an increase of aperture observation by nearly two order of magnitude (area-time by AGASA-HIRES-AUGER) no larger or equal event as eV has been rediscovered. Making wondering the nature of that exceptional starting UHECR event. To face the uncorrelated UHECR at eV, and later on event by AGASA, the earliest evidences (by SuperKamiokande) that neutrino have a non zero mass had opened [6] the possibility of an UHECR-Neutrino connection: UHE ZeV neutrino could be the transparent courier of a far AGN (beyond GZK radius) that may hit and scatter on a local relic anti-neutrino dark halo, spread at a few Mpc around our galaxy. Its resonant Z boson (or WW channel) production [6] is source of a secondary nucleon later on observable at Earth as a UHECR. The later search by AGASA seemed to confirm the Fly’s Eye by events above eV and the puzzling absence of nearby expected GZK anisotropy or correlation. On we were all convinced on the UHECR GZK cut absence. In different occasion HIRES data offered a possible UHECR connections with far BL Lac [13], giving argument to such Z-resonant (Z-burst) model. However more recent records by a larger Hires area (2001-2005) have been claiming evidences of GZK suppression in UHECR spectra. The same result seemed confirmed by last AUGER data in last few years [1]. But in addition AUGER have shown an anisotropic clustering, seeming along the Super Galactic Plane, a place well consistent with GZK expectation [1]. Because of it the UHE neutrino scattering model [6],) became obsolete.

Indeed here we review the most recent UHECR maps [3] over different Universe and we comment some feature, noting some possible minor galactic component [10], [12]. Moreover we remind possible Z-Showering model solution if UHECR are correlated to AGN,BLac or Quasars at large redshift. The consequences of the UHECR composition and source reflects into UHE (GZK [15] or cosmo-genic) neutrinos. The proton UHECR provide EeV neutrinos (muons and electron) whose flavor oscillation lead to tau neutrinos to be soon detectable [7] [2] by upward tau air-showers; the UHECR lightest nuclei model provide only lower energy, tens PeV, neutrinos detectable in a very peculiar way by AUGER fluorescence telescopes or in ARGO array by horizontal air-showers , or by Icecube neutrino telescopes [7],[11],[9] [10] either by double bang[16], or by long muon at few PeV energy. ZeV UHE neutrinos in Z-Shower model are possible source of horizontal Tau air-showers of maximal size and energy [7],[12].

1.1 The Lorentz UHECR bending and spread

Cosmic Rays are blurred by magnetic fields. Also UHECR suffer of a Lorentz force deviation. This smearing maybe source of UHECR features. Mostly along Cen A. There are two main spectroscopy of UHECR along galactic plane: A late nearby (almost local) bending by a nearest coherent galactic arm field, and a random one along the whole plane inside different arms. The coherent Lorentz angle bending of a proton UHECR (above GZK [15]) within a galactic magnetic field in a final nearby coherent length of is . The corresponding coherent bending of an Helium UHECR at same energy, within a galactic magnetic field in a wider nearby coherent length of is

(1)

This bending angle is compatible with observed multiplet along and also the possible clustering along Vela, at much nearer distances; indeed in latter case it is possible for a larger magnetic field along its direction (20 ) and-or for a rare iron composition . Such iron UHECR are mostly bounded inside a Galaxy, as well as in Virgo, explaining partially its extragalactic absence. In lightest nuclei model the rare heavier iron nuclei may be bounded inside Virgo. The incoherent random angle bending, , while crossing along the whole Galactic disk in different spiral arms and within a characteristic coherent length for He nuclei is The heavier (but still lightest nuclei) bounded from Virgo are Li and Be: , . It should be noted that the present anisotropy above GZK [15] energy might leave a tail of signals: indeed the photo disruption of He into deuterium, Tritium, and protons (and unstable neutrons), might rise as clustered events at half or a fourth of the energy: being with a fourth an energy but half a charge proton tails will smear around Cen-A at twice larger angle. It is important to look for correlated tails of events, possibly in strings at low along the train of events. It should be noticed that Deuterium fragments are half energy and mass of Helium: Therefore D and He spot are bent at same way and overlap into UHECR circle clusters. Deuterium are even more bounded in a local Universe because their fragility. In conclusion He like UHECR maybe bent by a characteristic as large as ,( its expected lower energy proton tails at ). Well within the observed CenA UHECR clustering spread.

Figure 1: The last 2010 UHECR event map by AUGER and the clustering toward Cen A, nearest AGN-Jet
Figure 2: The last 2010 UHECR event map by AUGER and the most recent Two Micron All Sky Survey (2MASS); it is remarkable the Virgo absence also in view of most recent TA and HIRES data. The cosmic Universe inside GZK volume do not correlate much with UHECR out of nearest Cen-A AGN and partial galactic possible components.
Figure 3: A first hint of Vela as a UHECR in celestial coordinated . The 69 Auger events (red-gray disks) are also shown with the 13 Hires (blue-black disk) UHECR events; note Virgo absence, note the clustering along Cen-A. Note the TeVs CR clustering around Vela, the brightest Gamma source in our galaxy with a triplet UHECR along.
Figure 4: The gamma Osse (Compton Observatory) map (1-3 MeV energy band) with the 69 UHECR of AUGER. This MeV background radiation is mostly of galactic sources as isotopes of titanium (Ti-44) and aluminum (Al-26), which are both produced in supernova explosions. Other sources are (AGN), which are massive black holes mostly (excluding CenA) at distances much larger than GZK. The clustering around CenA and the triplet around Vela, are correlated both in Comptel map; Vela triplet is correlated with new 12 TeV muon anisotropy discovered by IceCube [17].
Figure 5: The last UHECR AUGER Composition derived by air shower slant depth ; note the best fit of He on most of the highest UHECR events
Figure 6: The last UHECR Telescope Array Composition derived by air shower slant depth shown in RICAP 2011; note the best fit of He on most of the highest UHECR events
Figure 7: The very recent Flare from far AGN blazar , at half the Universe distance in Fermi sky and with UHECR. Its relevance is not just related to the huge output of the source and to the doublet AUGER event connected by this map: but also to additional signals. The Z-resonant (or Z-Burst) model explains this otherwise mysterious connection. The UHE neutrino primary energy need to be nearly ZeV and the relic neutrino mass might range in the eV. The whole conversion efficiency might range from a minimal [6] for no relic neutrino clustering up to a (forty) times density contrast in Local Group halo. Even within the minimal conversion efficiency, observed gamma flaring blazar is consistent with the extreme UHECR flux assuming a primary Fermi flat spectra (of the blazar) extending up to ZeV energy. See [6].Other AGN or Vela correlation are drawn by oval rings.

2 Conclusions: UHECR and UHE neutrinos

The history of Cosmic Rays and last UHECR discoveries (and disclaims) are exciting and surprising. The very surprising correlation with Cen A, the absence of Virgo, the hint of correlation with Vela and galactic center might be solved by a lightest nuclei, mainly He, as a courier, leading to a very narrow (few Mpc) sky for UHECR. However the very exceptional blazar flare on , the few AGN connection of UHECR located much far from a GZK distances may force us, surprisingly, to reconsider an exceptional model: Z-Shower one [6]. Possibly connecting lowest neutrino particle ( eV) mass with highest UHE (ZeV)neutrino energies. Even for the minimal UHE -Z-UHECR conversion as low as (see table,last reference in[6]), for a not clustered relic neutrino halo as diluted as cosmic ones the present gamma output (above ) is comparable with UHECR (two events in in AUGER), assuming a flat Fermi spectra (for neutrinos) extended up to UHECR ZeVs edges. These results are somehow surprising and revolutionary. We might be warned for unexpected very local and a very wide Universe sources sending UHECR traces in different ways. Testing finally the most evanescent hot neutrino relic background. The consequences may be soon detectable in different way by Tau air-showers in AUGER,TA, Heat and also in unexpected horizontal shower in deep valley by ARGO [7],[2] or in widest atmosphere layer on Earth, Jupiter and Saturn, see papers in[6]. A soon answer maybe already written into present clustering (as Deuterium fragments) at half UHECR edge energy around or along main UHECR group seed. Indeed He like UHECR maybe bent by a characteristic as large as ,(while expected proton at half fourth these energies, along tails spread at ). The next release of UHECR update events, possibly above 2-3 tens EeV, their fragment clustering maps along higher energy UHECR (5-6 eV) may solve the puzzles. As well the eventual revolutionary discover of an horizontal tau airshower nearby (by tau neutrinos at PeVs by UHECR light nuclei photo-dissociations) observed by ARGO; or by near (PeVs) or far (EeV) tau airshowers observed from fluorescence Auger and TA telescopes [10].

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