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000426141 0247_ $$2doi$$a10.1109/NSSMIC.2018.8824640
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000426141 041__ $$aEnglish
000426141 1001_ $$0P:(DE-HGF)0$$aRuz, J.$$b0$$eCorresponding author
000426141 1112_ $$a2018 IEEE Nuclear Science Symposium and Medical Imaging Conference (NSS/MIC)$$cSydney$$d2018-11-10 - 2018-11-17$$wAustralia
000426141 245__ $$aNext Generation Search for Axion and ALP Dark Matter with the International Axion Observatory
000426141 260__ $$bIEEE$$c2018
000426141 29510 $$a2018 IEEE Nuclear Science Symposium and Medical Imaging Conference Proceedings (NSS/MIC) - IEEE, 2018. - ISBN 978-1-5386-8494-8 - doi:10.1109/NSSMIC.2018.8824640
000426141 300__ $$a1-4
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000426141 520__ $$aMore than 80 years after the postulation of dark matter, its nature remains one of the fundamental questions in cosmology. Axions are currently one of the leading candidates for the hypothetical, non-baryonic dark matter that is expected to account for about 25% of the energy density of the Universe. Especially in the light of the Large Hadron Collider at CERN slowly closing in on Weakly-Interacting Massive Particle (WIMP) searches, axions and axion-like particles (ALPs) provide a viable alternative approach to solving the dark matter problem. The fact that makes them particularly appealing is that they were initially introduced to solve a long-standing problem in quantum chromodynamics and the Standard Model of particle physics.Helioscopes are a type of axion experiment searching for axions produced in the core of the Sun via the Primakoff effect. The International Axion Observatory (IAXO) is a next generation axion helioscope aiming at a sensitivity to the axion-photon coupling of 1 − 1.5 orders of magnitude beyond the current most sensitive axion helioscope, which is the CERN Axion Solar Telescope (CAST). IAXO will be able to challenge the stringent bounds from supernova SN1987A and test the axion interpretation of anomalous white-dwarf cooling. Beyond standard axions, this new experiment will also be able to search for a large variety of axion-like particles and other novel excitations at the low-energy frontier of elementary particle physics. BabyIAXO is proposed as an intermediate-scale experiment increasing the sensitivity to axion-photon couplings down to a few 10−11GeV−1and thus delivering significant physics results while demonstrating the feasibility of the full-scale IAXO experiment. Here we introduce the IAXO and BabyIAXO experiments, report on the current status of both and outline the expected IAXO science reach.
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000426141 7001_ $$aVogel, J. K.$$b1
000426141 7001_ $$aArmengaud, E.$$b2
000426141 7001_ $$0P:(DE-HGF)0$$aAttie, D.$$b3
000426141 7001_ $$aBasso, S.$$b4
000426141 7001_ $$aBrun, P.$$b5
000426141 7001_ $$aBykovskiy, N.$$b6
000426141 7001_ $$aCarmona, J. M.$$b7
000426141 7001_ $$aCastel, J. F.$$b8
000426141 7001_ $$aCebrian, S.$$b9
000426141 7001_ $$aCivitani, M.$$b10
000426141 7001_ $$aCogollos, C.$$b11
000426141 7001_ $$aCosta, D.$$b12
000426141 7001_ $$aDafni, T.$$b13
000426141 7001_ $$aDerbin, A. V.$$b14
000426141 7001_ $$aDescalle, M. A.$$b15
000426141 7001_ $$aDesch, K.$$b16
000426141 7001_ $$0P:(DE-HGF)0$$aDobrich, B.$$b17
000426141 7001_ $$aDratchnev, I.$$b18
000426141 7001_ $$aDudarev, A.$$b19
000426141 7001_ $$aFerrer-Ribas, E.$$b20
000426141 7001_ $$aGalan, J.$$b21
000426141 7001_ $$aGalanti, G.$$b22
000426141 7001_ $$0P:(DE-HGF)0$$aGascon, D.$$b23
000426141 7001_ $$aGastaldo, L.$$b24
000426141 7001_ $$aGarrido, L.$$b25
000426141 7001_ $$0P:(DE-HGF)0$$aGermani, C.$$b26
000426141 7001_ $$aGhisellini, G.$$b27
000426141 7001_ $$aGiannotti, M.$$b28
000426141 7001_ $$aGiomataris, I.$$b29
000426141 7001_ $$aGninenko, S.$$b30
000426141 7001_ $$aGolubev, N.$$b31
000426141 7001_ $$aGraciani, R.$$b32
000426141 7001_ $$aIrastorza, I. G.$$b33
000426141 7001_ $$aJakovcic, K.$$b34
000426141 7001_ $$0P:(DE-HGF)0$$aKaminski, J.$$b35
000426141 7001_ $$aKrcmar, M.$$b36
000426141 7001_ $$0P:(DE-HGF)0$$aKrieger, C.$$b37
000426141 7001_ $$aLakic, B.$$b38
000426141 7001_ $$aLasserre, T.$$b39
000426141 7001_ $$aLaurent, P.$$b40
000426141 7001_ $$aLomskaya, I.$$b41
000426141 7001_ $$aUnzhakov, E.$$b42
000426141 7001_ $$aLimousin, O.$$b43
000426141 7001_ $$0P:(DE-H253)PIP1003168$$aLindner, Axel$$b44
000426141 7001_ $$aLuzon, G.$$b45
000426141 7001_ $$aMescia, F.$$b46
000426141 7001_ $$aMiralda-Escude, J.$$b47
000426141 7001_ $$aMirallas, H.$$b48
000426141 7001_ $$aMuratova, V. N.$$b49
000426141 7001_ $$aNavick, X. F.$$b50
000426141 7001_ $$aNones, C.$$b51
000426141 7001_ $$aNotari, A.$$b52
000426141 7001_ $$aNozik, A.$$b53
000426141 7001_ $$aNunez, A.$$b54
000426141 7001_ $$aSolorzano, A. Ortiz de$$b55
000426141 7001_ $$aPantuev, V.$$b56
000426141 7001_ $$aPapaevangelou, T.$$b57
000426141 7001_ $$aPareschi, G.$$b58
000426141 7001_ $$aPicatoste, E.$$b59
000426141 7001_ $$aPivovaroff, M. J.$$b60
000426141 7001_ $$aPerez, K.$$b61
000426141 7001_ $$0P:(DE-HGF)0$$aRedondo, J.$$b62
000426141 7001_ $$0P:(DE-H253)PIP1001650$$aRingwald, A.$$b63
000426141 7001_ $$aRuiz-Choliz, E.$$b64
000426141 7001_ $$aSalvado, J.$$b65
000426141 7001_ $$aSchiffer, T.$$b66
000426141 7001_ $$0P:(DE-HGF)0$$aSchmidt, S.$$b67
000426141 7001_ $$0P:(DE-H253)PIP1001589$$aSchneekloth, U.$$b68$$udesy
000426141 7001_ $$0P:(DE-HGF)0$$aSchott, M.$$b69
000426141 7001_ $$0P:(DE-HGF)0$$aSilva, H.$$b70
000426141 7001_ $$aTagliaferri, G.$$b71
000426141 7001_ $$aTavecchio, F.$$b72
000426141 7001_ $$aKate, H. ten$$b73
000426141 7001_ $$aTkackev, I.$$b74
000426141 7001_ $$aTroitsky, S.$$b75
000426141 7001_ $$aVedrine, P.$$b76
000426141 7001_ $$aWeltman, A.$$b77
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