MULTIWAVELENGTH STUDY OF QUIESCENT STATES OF Mrk 421 WITH UNPRECEDENTED HARD X-RAY COVERAGE PROVIDED BY NuSTAR IN 2013

被引：95

作者：

Balokovic, M. ^{[1
]}

Paneque, D. ^{[2
]}

Madejski, G. ^{[3
,4
]}

Furniss, A. ^{[5
]}

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

Ajell, M. ^{[6
]}

Alexander, D. M. ^{[7
]}

Barret, D. ^{[8
,9
]}

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

Boggs, S. E. ^{[10
]}

Christensen, F. E. ^{[11
]}

Craig, W. W. ^{[10
,12
]}

Forster, K. ^{[1
]}

Giommi, P. ^{[13
]}

Grefenstette, B. ^{[1
]}

Hailey, C. ^{[14
]}

Harrison, F. A. ^{[1
]}

Hornstrup, A. ^{[11
]}

Kitaguchi, T. ^{[15
,16
]}

Koglin, J. E. ^{[3
,4
]}

Madsen, K. K. ^{[1
]}

Mao, P. H. ^{[1
]}

Miyasaka, H. ^{[1
]}

Mori, K. ^{[17
]}

Perri, M. ^{[13
,18
]}

Pivovaroff, M. J. ^{[10
]}

Puccetti, S. ^{[13
,18
]}

Rana, V. ^{[1
]}

Stern, D. ^{[19
]}

Tagliaferri, G. ^{[20
]}

Urry, C. M. ^{[21
]}

Estergaard, N. J. W. ^{[11
]}

Zhang, W. W. ^{[22
]}

Zoglauer, A. ^{[10
]}

Archambault, S. ^{[23
]}

Archer, A. ^{[24
]}

Barnacka, A. ^{[25
]}

Benbow, W. ^{[26
]}

Bird, R. ^{[27
]}

Buckley, J. H. ^{[24
]}

Bugaev, V. ^{[24
]}

Cerruti, M. ^{[26
]}

Chen, X. ^{[28
,29
]}

Ciupik, L. ^{[30
]}

Connolly, M. P. ^{[31
]}

Cui, W. ^{[32
]}

Dickinson, H. J. ^{[33
]}

Dumm, J. ^{[34
]}

Eisch, J. D. ^{[33
]}

Falcone, A. ^{[35
]}

机构：

[1] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA

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

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

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

[5] Stanford Univ, Dept Phys, Stanford, CA 94305 USA

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

[7] Univ Durham, Dept Phys, Durham DH1 3LE, England

[8] Univ Toulouse, UPS OMP, IRAP, Toulouse, France

[9] CNRS, Inst Rech Astrophys & Planetol, 9 Ave Colonel Roche,BP 44346, F-31028 Toulouse 4, France

[10] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA

[11] Tech Univ Denmark, Natl Space Inst, DTU Space, Elektrovej 327, DK-2800 Lyngby, Denmark

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

[13] ASI Sci Data Ctr, Via Politecn Snc, I-00133 Rome, Italy

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

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

[16] Hiroshima Univ, Core Res Energet Universe, Higashihiroshima, Hiroshima 7398526, Japan

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

[18] Osserv Astron Roma, INAF, Via Frascati 33, I-00040 Monte Porzio Catone, Italy

[19] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA

[20] Osservatorio Astronomico Brera, INAF, Via E Bianchi 46, I-23807 Merate, Italy

[21] Yale Univ, Dept Phys, Yale Ctr Astron & Astrophys, POB 208120, New Haven, CT 06520 USA

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

[23] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada

[24] Washington Univ, Dept Phys, St Louis, MO 63130 USA

[25] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA

[26] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA

[27] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland

[28] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany

[29] Deutsch Elektronen Synchrotron DESY, Platanenallee 6, D-15738 Zeuthen, Germany

[30] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA

[31] Natl Univ Ireland Galway, Sch Phys, Univ Rd, Galway, Ireland

[32] Purdue Univ, Dept Phys & Astron, W Lafayette, IN 47907 USA

[33] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA

[34] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA

[35] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA

[36] Univ Iowa, Dept Phys & Astron, Van Allen Hall, Iowa City, IA 52242 USA

[37] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA

[38] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA

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

[40] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA

[41] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA

[42] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA

[43] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA

[44] Georgia Inst Technol, Sch Phys, 837 State St NW, Atlanta, GA 30332 USA

[45] Georgia Inst Technol, Ctr Relativist Astrophys, 837 State St NW, Atlanta, GA 30332 USA

[46] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA

[47] Cork Inst Technol, Dept Appl Sci, Cork, Ireland

[48] Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA

[49] Univ Maryland, College Pk, MD 20742 USA

[50] Argonne Natl Lab, 9700 S Cass Ave, Argonne, IL 60439 USA

来源：

ASTROPHYSICAL JOURNAL | 2016年 / 819卷 / 02期

基金：

美国国家科学基金会; 芬兰科学院; 加拿大自然科学与工程研究理事会; 新加坡国家研究基金会; 美国国家航空航天局;

关键词：

BL Lacertae objects: individual (Markarian 421); galaxies: active; gamma rays: general; radiation mechanisms: nonthermal; X-rays: galaxies; LARGE-AREA TELESCOPE; PARTICLE-ACCELERATION; TEV BLAZARS; CORRELATED VARIABILITY; ELECTRON ACCELERATION; BACKGROUND-RADIATION; SWIFT OBSERVATIONS; LAC OBJECTS; 3C; 454.3; RADIO;

D O I：

10.3847/0004-637X/819/2/156

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present coordinated multiwavelength observations of the bright, nearby BL Lacertae object Mrk 421 taken in 2013 January-March, involving GASP-WEBT, Swift, NuSTAR, Fermi-LAT, MAGIC, VERITAS, and other collaborations and instruments, providing data from radio to very high energy. (VHE).-ray bands. NuSTAR yielded previously unattainable sensitivity in the 3-79. keV range, revealing that the spectrum softens when the source is dimmer until the X-ray spectral shape saturates into a steep Gamma approximate to 3 power law, with no evidence for an exponential cutoff or additional hard components up to similar to 80. keV. For the first time, we observed both the synchrotron and the inverse-Compton peaks of the spectral energy distribution (SED) simultaneously shifted to frequencies below the typical quiescent state by an order of magnitude. The fractional variability as a function of photon energy shows a double-bump structure that relates to the two bumps of the broadband SED. In each bump, the variability increases with energy, which, in the framework of the synchrotron self-Compton model, implies that the electrons with higher energies are more variable. The measured multi band variability, the significant X-ray-to-VHE correlation down to some of the lowest fluxes ever observed in both bands, the lack of correlation between optical/UV and X-ray flux, the low degree of polarization and its significant (random) variations, the short estimated electron cooling time, and the significantly longer variability timescale observed in the NuSTAR light curves point toward in situ electron acceleration and suggest that there are multiple compact regions contributing to the broadband emission of Mrk 421 during low-activity states.

引用

页数：30

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