FERMI OBSERVATIONS OF γ-RAY EMISSION FROM THE MOON

被引：22

作者：

Abdo, A. A.

Ackermann, M. ^{[2
]}

Ajello, M. ^{[3
,4
]}

Atwoo, W. B. ^{[5
,6
]}

Baldini, L. ^{[7
]}

Ballet, J. ^{[8
]}

Barbiellini, G. ^{[9
,10
]}

Bastieri, D. ^{[11
]}

Bechtol, K. ^{[3
,4
]}

Bellazzini, R. ^{[7
]}

Berenji, B. ^{[3
,4
]}

Blandford, R. D. ^{[3
,4
]}

Bonamente, E. ^{[12
,13
]}

Borgland, A. W. ^{[3
,4
]}

Bottacini, E. ^{[3
,4
]}

Bouvier, A. ^{[4
,5
,6
]}

Bregeon, J. ^{[7
]}

Brigida, M. ^{[14
,15
]}

Bruel, P. ^{[16
]}

Buehler, R. ^{[3
,4
]}

Buson, S. ^{[11
]}

Caliandro, G. A. ^{[17
]}

Cameron, R. A. ^{[3
,4
]}

Caraveo, P. A. ^{[18
]}

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

Cecchi, C. ^{[12
,13
]}

Charles, E. ^{[3
,4
]}

Chekhtman, A. ^{[1
]}

Chiang, J. ^{[3
,4
]}

Ciprini, S. ^{[13
,19
]}

Claus, R. ^{[3
,4
]}

Cohen-Tanugi, J.

Conrad, J. ^{[20
,21
]}

Cutini, S.

D'Ammando, F. ^{[12
,22
,23
]}

de Angelis, A. ^{[24
,25
]}

de Palma, F. ^{[14
,15
]}

Dermer, C. D. ^{[26
]}

Digel, S. W. ^{[3
,4
]}

Silva, E. do Couto E ^{[3
,4
]}

Drell, P. S. ^{[3
,4
]}

Drlica-Wagner, A. ^{[3
,4
]}

Dubois, R. ^{[3
,4
]}

Favuzzi, C. ^{[14
,15
]}

Fegan, S. J. ^{[16
]}

Focke, W. B. ^{[3
,4
]}

Fortin, P. ^{[16
]}

Fukazawa, Y. ^{[27
]}

Funk, S. ^{[3
,4
]}

Fusco, P. ^{[14
,15
]}

机构：

[1] George Mason Univ, Ctr Earth Observing & Space Res, Coll Sci, Fairfax, VA 22030 USA

[2] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany

[3] Stanford Univ, Dept Phys, WW Hansen Expt Phys Lab, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA

[4] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA

[5] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA

[6] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA

[7] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy

[8] Univ Paris Diderot, Lab AIM, CNRS, CEA IRFU,CEA Saclay,Serv Astrophys, F-91191 Gif Sur Yvette, France

[9] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy

[10] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy

[11] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy

[12] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy

[13] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy

[14] Univ Politecn Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy

[15] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy

[16] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France

[17] CSIC, Inst Ciencies Espai IEEE, E-08193 Barcelona, Spain

[18] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy

[19] ASI Sci Data Ctr, I-00044 Frascati, Roma, Italy

[20] Stockholm Univ, AlbaNova, Dept Phys, SE-10691 Stockholm, Sweden

[21] AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden

[22] IASF Palermo, I-90146 Palermo, Italy

[23] INAF Ist Astrofis Spaziale & Fis Cosm, I-00133 Rome, Italy

[24] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy

[25] Ist Nazl Fis Nucl, Sez Trieste, Grp Collegato Udine, I-33100 Udine, Italy

[26] USN, Div Space Sci, Res Lab, Washington, DC 20375 USA

[27] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan

[28] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA

[29] INAF, Ist Radioastron, I-40129 Bologna, Italy

[30] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy

[31] Univ Autonoma Madrid, Dept Fis Teor, E-28049 Madrid, Spain

[32] Univ Autonoma Madrid, CSIC, UAM, IFT, E-28049 Madrid, Spain

[33] Univ Alabama, CSPAR, Huntsville, AL 35899 USA

[34] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England

[35] Univ Bordeaux 1, CNRS, IN2P3, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France

[36] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA

[37] Osserv Astron Trieste, Ist Nazl Astrofis, I-34143 Trieste, Italy

[38] Royal Inst Technol KTH, AlbaNova, Dept Phys, SE-10691 Stockholm, Sweden

[39] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland

[40] Ibaraki Univ, Coll Sci, Mito, Ibaraki 3108512, Japan

[41] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan

[42] CNRS, IRAP, F-31028 Toulouse 4, France

[43] Univ Toulouse, IRAP, UPS OMP, GAHEC, Toulouse, France

[44] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden

[45] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy

[46] Univ Bordeaux 1, Ctr Etud Nucl Bordeaux Gradignan, CNRS, IN2P3, F-33175 Gradignan, France

[47] Univ Maryland, Dept Phys, College Pk, MD 20742 USA

[48] Univ Maryland, Dept Astron, College Pk, MD 20742 USA

[49] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan

[50] CRESST, Greenbelt, MD 20771 USA

来源：

ASTROPHYSICAL JOURNAL | 2012年 / 758卷 / 02期

基金：

美国国家科学基金会;

关键词：

astroparticle physics; gamma rays: general; Moon; LARGE-AREA TELESCOPE; LUNAR-SURFACE; ELEMENTAL COMPOSITION; ALBEDO; SPECTROSCOPY; ASTRONOMY;

D O I：

10.1088/0004-637X/758/2/140

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We report on the detection of high-energy gamma-ray emission from the Moon during the first 24 months of observations by the Fermi Large Area Telescope (LAT). This emission comes from particle cascades produced by cosmic-ray (CR) nuclei and electrons interacting with the lunar surface. The differential spectrum of the Moon is soft and can be described as a log-parabolic function with an effective cutoff at 2-3 GeV, while the average integral flux measured with the LAT from the beginning of observations in 2008 August to the end of 2010 August is F(> 100 MeV) = (1.04 +/- 0.01 [statistical error] +/- 0.1 [systematic error]) x 10(-6) cm(-2) s(-1). This flux is about a factor 2-3 higher than that observed between 1991 and 1994 by the EGRET experiment on board the Compton Gamma Ray Observatory, F(> 100 MeV) approximate to 5 x 10(-7) cm-2 s-1, when solar activity was relatively high. The higher gamma-ray flux measured by Fermi is consistent with the deep solar minimum conditions during the first 24 months of the mission, which reduced effects of heliospheric modulation, and thus increased the heliospheric flux of Galactic CRs. A detailed comparison of the light curve with McMurdo Neutron Monitor rates suggests a correlation of the trends. The Moon and the Sun are so far the only known bright emitters of gamma-rays with fast celestial motion. Their paths across the sky are projected onto the Galactic center and high Galactic latitudes as well as onto other areas crowded with high-energy gamma-ray sources. Analysis of the lunar and solar emission may thus be important for studies of weak and transient sources near the ecliptic.

引用

页数：8

共 33 条

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