Search for Gamma-Ray Emission from Local Primordial Black Holes with the Fermi Large Area Telescope

被引：26

作者：

Ackermann, M. ^{[1
]}

Atwood, W. B. ^{[2
,3
]}

Baldini, L. ^{[4
,5
]}

Ballet, J. ^{[6
]}

Barbiellini, G. ^{[7
,8
]}

Bastieri, D. ^{[9
,10
]}

Bellazzini, R. ^{[11
]}

Berenji, B. ^{[12
]}

Bissaldi, E. ^{[13
,14
]}

Blandford, R. D. ^{[15
,16
]}

Bloom, E. D. ^{[15
,16
]}

Bonino, R. ^{[17
,18
]}

Bottacini, E. ^{[15
,16
]}

Bregeon, J. ^{[19
]}

Bruel, P. ^{[20
]}

Buehler, R. ^{[1
]}

Cameron, R. A. ^{[15
,16
]}

Caputo, R. ^{[21
,22
]}

Caraveo, P. A. ^{[23
]}

Cavazzuti, E. ^{[24
]}

Charles, E. ^{[15
,16
]}

Chekhtman, A. ^{[25
,26
]}

Cheung, C. C. ^{[27
]}

Chiaro, G. ^{[23
]}

Ciprini, S. ^{[28
,29
]}

Cohen-Tanugi, J.

Conrad, J. ^{[30
,31
]}

Costantin, D. ^{[10
]}

D'Ammando, F. ^{[32
,33
]}

de Palma, F. ^{[14
,34
]}

Digel, S. W. ^{[15
,16
]}

Di Lalla, N. ^{[4
,5
]}

Di Mauro, M. ^{[15
,16
]}

Di Venere, L. ^{[13
,14
]}

Favuzzi, C. ^{[13
,14
]}

Fegan, S. J. ^{[20
]}

Focke, W. B. ^{[15
,16
]}

Franckowiak, A. ^{[1
,13
]}

Fukazawa, Y. ^{[35
]}

Funk, S. ^{[36
]}

Fusco, P. ^{[13
,14
]}

Gargano, F. ^{[14
]}

Gasparrini, D. ^{[28
,29
]}

Giglietto, N. ^{[13
,14
]}

Giordano, F. ^{[13
,14
]}

Giroletti, M. ^{[32
]}

Green, D. ^{[37
,38
,39
]}

Grenier, I. A. ^{[6
]}

Guillemot, L. ^{[40
,41
]}

Guiriec, S. ^{[39
,42
]}

机构：

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

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

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

[4] Univ Pisa, I-56127 Pisa, Italy

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

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

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

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

[9] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy

[10] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy

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

[12] Calif State Univ Los Angeles, Dept Phys & Astron, Los Angeles, CA 90032 USA

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

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

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

[16] Stanford Univ, Natl Accelerator Lab, Stanford, CA 94305 USA

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

[18] Univ Torino, Dipartimento Fis, I-10125 Turin, Italy

[19] Univ Montpellier, CNRS IN2P3, Lab Univers & Particules Montpellier, F-34095 Montpellier, France

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

[21] CRESST, Greenbelt, MD 20771 USA

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

[23] INAF Ist Astrofis Spaziale & Fis Cosm Milano, Via E Bassini 15, I-20133 Milan, Italy

[24] Italian Space Agcy, Via Politecn Snc, I-00133 Rome, Italy

[25] George Mason Univ, Coll Sci, Fairfax, VA 22030 USA

[26] US Navy, Res Lab, Washington, DC 20375 USA

[27] US Navy, Res Lab, Space Sci Div, Washington, DC 20375 USA

[28] Agenzia Spaziale Italiana, Space Sci Data CenteR, Via Politecn, I-00133 Rome, Italy

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

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

[31] AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, S-10691 Stockholm, Sweden

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

[33] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy

[34] Univ Telemat Pegaso, Piazza Trieste & Trento 48, I-80132 Naples, Italy

[35] Hiroshima Univ, Dept Phys Sci, Higashihiroshima, Hiroshima 7398526, Japan

[36] Friedrich Alexander Univ Erlangen Nurnberg, Erlangen Ctr Astroparticle Phys, Erwin Rommel Str 1, D-91058 Erlangen, Germany

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

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

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

[40] Univ Orleans, CNRS, Lab Phys & Chim Environnement & Espace, F-45071 Orleans 02, France

[41] INSU, Observ Paris, CNRS, Stn Radioastron Nancay, F-18330 Nancay, France

[42] George Washington Univ, Dept Phys, 725 21st St, Washington, DC 20052 USA

[43] Univ Iceland, Inst Sci, IS 107, Reykjavik, Iceland

[44] NORDITA, Roslagstullsbacken 23, SE-10691 Stockholm, Sweden

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

[46] Inst Space Sci CSICIEEC, Campus UAB,Carrer Magrans S-N, E-08193 Barcelona, Spain

[47] Mahidol Univ, Fac Sci, Dept Phys, Bangkok 10400, Thailand

[48] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Higashihiroshima, Hiroshima 7398526, Japan

[49] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany

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

来源：

ASTROPHYSICAL JOURNAL | 2018年 / 857卷 / 01期

关键词：

astroparticle physics; black hole physics; methods: data analysis; GLUON-JET EMISSION; COSMIC-RAYS; MILKY-WAY; QUARK-JET; MASS; EXPLOSIONS; HALO; CONSTRAINTS; DENSITY; BURSTS;

D O I：

10.3847/1538-4357/aaac7b

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Black holes with masses below approximately 10(15) g are expected to emit gamma-rays with energies above a few tens of MeV, which can be detected by the Fermi Large Area Telescope (LAT). Although black holes with these masses cannot be formed as a result of stellar evolution, they may have formed in the early universe and are therefore called primordial black holes (PBHs). Previous searches for PBHs have focused on either short-timescale bursts or the contribution of PBHs to the isotropic gamma-ray emission. We show that, in cases of individual PBHs, the Fermi-LAT is most sensitive to PBHs with temperatures above approximately 16 GeV and masses 6 x 10(11) g, which it can detect out to a distance of about 0.03 pc. These PBHs have a remaining lifetime of months to years at the start of the Fermi mission. They would appear as potentially moving point sources with gamma-ray emission that become spectrally harder and brighter with time until the PBH completely evaporates. In this paper, we develop a new algorithm to detect the proper motion of gamma-ray point sources, and apply it to 318 unassociated point sources at a high galactic latitude in the third Fermi-LAT source catalog. None of the unassociated point sources with spectra consistent with PBH evaporation show significant proper motion. Using the nondetection of PBH candidates, we derive a 99% confidence limit on the PBH evaporation rate in the vicinity of Earth, <(rho)over dot>(PBH) < 7.2 x 10(3) pc(-3) yr(-1). This limit is similar to the limits obtained with ground-based gamma-ray observatories.

引用

页数：11

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