Improved search for solar chameleons with a GridPix detector at CAST

被引：12

作者：

Anastassopoulos, V ^{[1
]}

Aune, S. ^{[2
]}

Barth, K. ^{[3
]}

Belov, A. ^{[4
]}

Braueninger, H. ^{[5
]}

Cantatore, G. ^{[6
,7
]}

Carmona, J. M. ^{[8
]}

Castel, J. F. ^{[8
]}

Cetin, S. A. ^{[9
]}

Christensen, F. ^{[10
]}

Dafni, T. ^{[8
]}

Davenport, M. ^{[3
]}

Dermenev, A. ^{[4
]}

Desch, K. ^{[11
]}

Doebrich, B. ^{[3
]}

Eleftheriadis, C. ^{[12
]}

Fanourakis, G. ^{[13
]}

Ferrer-Ribas, E. ^{[2
]}

Fischer, H. ^{[14
]}

Funk, W. ^{[3
]}

Garcia, J. A. ^{[8
,31
]}

Gardikiotis, A. ^{[1
]}

Garza, J. G. ^{[8
]}

Gazis, E. N. ^{[15
]}

Geralis, T. ^{[13
]}

Giomataris, I ^{[2
]}

Gninenko, S. ^{[4
]}

Hailey, C. J. ^{[16
,17
]}

Hasinoff, M. D. ^{[18
]}

Hoffmann, D. H. H. ^{[19
]}

Iguaz, F. J. ^{[8
]}

Irastorza, I. G. ^{[8
]}

Jakobsen, A. ^{[10
]}

Jacoby, J. ^{[20
]}

Jakovcic, K. ^{[21
]}

Kaminski, J. ^{[11
]}

Karuza, M. ^{[22
,23
]}

Kostoglou, S. ^{[3
]}

Kralj, N. ^{[22
,23
,32
]}

Krcmar, M. ^{[21
]}

Krieger, C. ^{[11
,33
]}

Lakic, B. ^{[21
]}

Laurent, J. M. ^{[3
]}

Liolios, A. ^{[12
]}

Ljubicic, A. ^{[21
]}

Luzon, G. ^{[8
]}

Maroudas, M. ^{[1
]}

Miceli, L. ^{[24
]}

Neff, S. ^{[25
]}

Ortega, I ^{[3
,8
]}

机构：

[1] Univ Patras, Phys Dept, Patras, Greece

[2] Univ Paris Saclay, CEA, IRFU, Gif Sur Yvette, France

[3] CERN, European Org Nucl Res, Geneva, Switzerland

[4] Russian Acad Sci, INR, Moscow, Russia

[5] Max Planck Inst Extraterr Phys, Garching, Germany

[6] INFN, Sez Trieste, Trieste, Italy

[7] Univ Trieste, Trieste, Italy

[8] Univ Zaragoza, Grp Invest Fis Nucl & Astroparticulas, Zaragoza, Spain

[9] Istanbul Bilgi Univ, High Energy Phys Res Ctr, Eyup, TR-34060 Istanbul, Turkey

[10] Tech Univ Denmark, Natl Space Inst, DTU Space, Lyngby, Denmark

[11] Univ Bonn, Phys Inst, Bonn, Germany

[12] Aristotle Univ Thessaloniki, Thessaloniki, Greece

[13] Natl Ctr Sci Res Demokritos, Athens, Greece

[14] Albert Ludwigs Univ Freiburg, Freiburg, Germany

[15] Natl Tech Univ Athens, Athens, Greece

[16] Columbia Univ, Phys Dept, New York, NY 10027 USA

[17] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA

[18] Univ British Columbia, Dept Phys & Astron, Vancouver, BC, Canada

[19] Xi An Jiao Tong Univ, Sch Sci, Xian, Shaanxi, Peoples R China

[20] Goethe Univ Frankfurt, Inst Angew Phys, Frankfurt, Germany

[21] Rudjer Boskovic Inst, Zagreb, Croatia

[22] Univ Rijeka, Dept Phys, Rijeka, Croatia

[23] Univ Rijeka, Ctr Micro & Nano Sci & Technol, Rijeka, Croatia

[24] Inst for Basic Sci Korea, Ctr Axion & Precis Phys Res, Daejeon 34141, South Korea

[25] Tech Univ Darmstadt, IKP, Darmstadt, Germany

[26] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA

[27] Max Planck Inst Phys & Astrophys, Werner Heisenberg Inst, Munich, Germany

[28] Korea Adv Inst Sci & Technol, Dept Phys, Daejeon 34141, South Korea

[29] Max Planck Inst Sonnensystemforsch, Gottingen, Germany

[30] Inst Phys Theor, CNRS, IPhT, CEA,URA 2306, F-91191 Gif Sur Yvette, France

[31] Chinese Acad Sci, Inst High Energy Phys, Beijing, Peoples R China

[32] Yale Univ, Dept Phys, New Haven, CT 06511 USA

[33] Univ Hamburg, Inst Expt Phys, Hamburg, Germany

[34] Extreme Light Infrastruct Nucl Phys ELI NP, Magurele 077125, Romania

[35] Kyung Hee Univ, Sch Space Res, Yongin, South Korea

[36] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA

来源：

JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS | 2019年 / 01期

基金：

欧洲研究理事会; 加拿大自然科学与工程研究理事会; 美国国家科学基金会;

关键词：

dark energy experiments; modified gravity; particle physics - cosmology connection; solar physics; X-RAY-DETECTOR;

D O I：

10.1088/1475-7516/2019/01/032

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We report on a new search for solar chameleons with the CERN Axion Solar Telescope (CAST). A GridPix detector was used to search for soft X-ray photons in the energy range from 200 eV to 10 keV from converted solar chameleons. No significant excess over the expected background has been observed in the data taken in 2014 and 2015. We set an improved limit on the chameleon photon coupling, beta(gamma) less than or similar to 5.7 x 10(10) for 1 < beta(m) < 10(6) at 95% C.L. improving our previous results by a factor two and for the first time reaching sensitivity below the solar luminosity bound for tachocline magnetic fields up to 12.5 T.

引用

页数：18

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