CONTEMPORANEOUS BROADBAND OBSERVATIONS OF THREE HIGH-REDSHIFT BL LAC OBJECTS

被引：5

作者：

Ackermann, M. ^{[1
]}

Ajello, M. ^{[2
]}

An, H. ^{[3
,4
]}

Baldini, L. ^{[3
,4
,5
,6
]}

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

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

Bellazzini, R. ^{[6
]}

Bissaldi, E. ^{[11
]}

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

Bonino, R. ^{[12
,13
]}

Bregeon, J. ^{[14
]}

Britto, R. J. ^{[15
]}

Bruel, P. ^{[16
]}

Buehler, R. ^{[1
]}

Caliandro, G. A. ^{[3
,4
,17
]}

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

Caragiulo, M. ^{[11
,18
]}

Caraveo, P. A. ^{[19
]}

Cavazzuti, E. ^{[20
]}

Cecchi, C. ^{[21
,22
]}

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

Chekhtman, A. ^{[6
,23
,24
]}

Chiaro, G. ^{[10
]}

Ciprini, S. ^{[20
,21
]}

Cohen-Tanugi, J. ^{[14
]}

Costanza, F. ^{[11
]}

Cutini, S. ^{[20
,21
,25
]}

D'Ammando, F. ^{[26
,27
]}

de Angelis, A. ^{[28
,29
]}

de Palma, F. ^{[11
,30
]}

Desiante, R. ^{[12
,31
]}

Di Mauro, M. ^{[3
,4
]}

Di Venere, L. ^{[11
,18
]}

Dominiguez, A. ^{[2
]}

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

Favuzzi, C. ^{[11
,18
]}

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

Ferrara, E. C. ^{[32
]}

Finke, J. ^{[33
]}

Fusco, P. ^{[11
,18
]}

Gargano, F. ^{[11
]}

Gasparrini, D. ^{[20
,21
]}

Giglietto, N. ^{[11
,18
]}

Giordano, F. ^{[11
,18
]}

Giroletti, M. ^{[26
]}

Green, D. ^{[32
,34
,35
]}

Grenier, I. A. ^{[36
]}

Guiriec, S. ^{[32
]}

Horan, D. ^{[16
]}

Johannesson, G. ^{[37
]}

机构：

[1] DESY, Deutsch Elekt Synchrotron, D-12738 Zeuthen, Germany

[2] Clemson Univ, Dept Phys & Astron, Kinard Lab Phys, Clemson, SC 29634 USA

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

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

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

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

[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 Bari, I-70126 Bari, Italy

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

[13] Univ Turin, Dipartimento Fis Gen Amadeo Avogadro, I-10125 Turin, Italy

[14] Univ Montpellier, Lab Univ & Particules Montpellier, CNRS, IN2P3, F-34059 Montpellier, France

[15] Univ Johannesburg, Dept Phys, POB 524,Auckland Pk, ZA-2006 Johannesburg, South Africa

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

[17] CIFS, I-10133 Turin, Italy

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

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

[20] ASI Sci Data Ctr, I-00133 Rome, Italy

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

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

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

[24] Naval Res Lab, Washington, DC 20375 USA

[25] Osserv Astron Roma, INAF, I-00040 Rome, Italy

[26] Inst Radioastron, INAF, I-40129 Bologna, Italy

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

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

[29] Ist Nazl Fis Nucl, Sez Trieste, Grp Coll Udine, I-33100 Udine, Italy

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

[31] Univ Udine, I-33100 Udine, Italy

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

[33] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA

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

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

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

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

[38] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2525210, Japan

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

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

[41] Inst Space Sci IEEC CSIC, Campus UAB, E-08193 Barcelona, Spain

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

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

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

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

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

[47] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria

[48] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria

[49] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany

[50] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA

来源：

ASTROPHYSICAL JOURNAL | 2016年 / 820卷 / 01期

基金：

美国国家航空航天局;

关键词：

BL Lacertae objects: general; BL Lacertae objects: individual (3FGL J0022.1-1855; 3FGL J0630.9-2406; 3FGL J0811.2-7529); galaxies: active; radiation mechanisms: non-thermal; EXTRAGALACTIC BACKGROUND LIGHT; LARGE-AREA TELESCOPE; SPECTRAL ENERGY-DISTRIBUTION; MULTIWAVELENGTH OBSERVATIONS; PHYSICAL-PROPERTIES; RAY-ABSORPTION; EVOLUTION; SAMPLE; SPECTROSCOPY; POLARIZATION;

D O I：

10.3847/0004-637X/820/1/72

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We have collected broadband spectral energy distributions (SEDs) of three BL Lac objects 3FGL J0022.1-1855 (z = 0.689), 3FGL J0630.9-2406 (z greater than or similar to 1.239), and 3FGL J0811.2-7529 (z = 0.774), detected by Fermi with relatively flat gigaelectronvolt spectra. By observing simultaneously in the near-infrared to hard X-ray band, we can well characterize the high end of the synchrotron component of the SED. Thus, fitting the SEDs to synchro-Compton models of the dominant emission from the relativistic jet, we can constrain the underlying particle properties and predict the shape of the gigaelectronvolt Compton component. Standard extragalactic background light (EBL) models explain the high-energy absorption well, with poorer fits for high-ultraviolet models. The fits show clear evidence for EBL absorption in the Fermi spectrum of our highest-redshift source 3FGL J0630.9-2406. While synchrotron self-Compton models adequately describe the SEDs, the situation may be complicated by possible external Compton components. For 3FGL J0811.2-7529, we also discover a nearby serendipitous source in the X-ray data, which is almost certainly another lower synchrotron peak frequency (nu(sy)(pk)) BL Lac, that may contribute flux in the Fermi band. Since our sources are unusual high-luminosity, moderate nu(sy)(pk) BL Lacs, we compare these quantities and the Compton dominance, the ratio of peak inverse Compton to peak synchrotron luminosities (L-pk(IC)/L-pk(sy)), with those of the full Fermi BL Lac population.

引用

页数：12

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