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Title: The structure and emission model of the relativistic jet in the quasar 3C 279 inferred from radio to high-energy γ-ray observations in 2008-2010

Abstract

Here, we present time-resolved broadband observations of the quasar 3C 279 obtained from multi-wavelength campaigns conducted during the first two years of the Fermi Gamma-ray Space Telescope mission. And, while investigating the previously reported γ-ray/optical flare accompanied by a change in optical polarization, we found that the optical emission appears to be delayed with respect to the γ-ray emission by about 10 days. X-ray observations reveal a pair of "isolated" flares separated by ~90 days, with only weak γ-ray/optical counterparts. The spectral structure measured by Spitzer reveals a synchrotron component peaking in the mid-infrared band with a sharp break at the far-infrared band during the γ-ray flare, while the peak appears in the millimeter (mm)/submillimeter (sub-mm) band in the low state. Selected spectral energy distributions are fitted with leptonic models including Comptonization of external radiation produced in a dusty torus or the broad-line region. Furthermore, by adopting the interpretation of the polarization swing involving propagation of the emitting region along a curved trajectory, we can explain the evolution of the broadband spectra during the γ-ray flaring event by a shift of its location from ~1 pc to ~4 pc from the central black hole. On the other hand, if themore » γ-ray flare is generated instead at sub-pc distance from the central black hole, the far-infrared break can be explained by synchrotron self-absorption. We also model the low spectral state, dominated by the mm/sub-mm peaking synchrotron component, and suggest that the corresponding inverse-Compton component explains the steady X-ray emission.« less

Authors:
; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; more »; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; ; « less
Publication Date:
Research Org.:
SLAC National Accelerator Lab., Menlo Park, CA (United States)
Sponsoring Org.:
USDOE
Contributing Org.:
Fermi LAT Collaboration
OSTI Identifier:
1356717
Grant/Contract Number:  
AC02-76SF00515
Resource Type:
Accepted Manuscript
Journal Name:
The Astrophysical Journal
Additional Journal Information:
Journal Volume: 754; Journal Issue: 2; Journal ID: ISSN 0004-637X
Publisher:
Institute of Physics (IOP)
Country of Publication:
United States
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS; galaxies: active; galaxies: jets; gamma rays: galaxies; quasars: individual (3C 279); radiation mechanisms: non-thermal; x-rays: galaxies

Citation Formats

Hayashida, M., Madejski, G. M., Nalewajko, K., Sikora, M., Wehrle, A. E., Ogle, P., Collmar, W., Larsson, S., Fukazawa, Y., Itoh, R., Chiang, J., Stawarz, Ł., Blandford, R. D., Richards, J. L., Max-Moerbeck, W., Readhead, A., Buehler, R., Cavazzuti, E., Ciprini, S., Gehrels, N., Reimer, A., Szostek, A., Tanaka, T., Tosti, G., Uchiyama, Y., Kawabata, K. S., Kino, M., Sakimoto, K., Sasada, M., Sato, S., Uemura, M., Yamanaka, M., Greiner, J., Kruehler, T., Rossi, A., Macquart, J. P., Bock, D. C. -J., Villata, M., Raiteri, C. M., Agudo, I., Aller, H. D., Aller, M. F., Arkharov, A. A., Bach, U., Benítez, E., Berdyugin, A., Blinov, D. A., Blumenthal, K., Böttcher, M., Buemi, C. S., Carosati, D., Chen, W. P., Paola, A. Di, Dolci, M., Efimova, N. V., Forné, E., Gómez, J. L., Gurwell, M. A., Heidt, J., Hiriart, D., Jordan, B., Jorstad, S. G., Joshi, M., Kimeridze, G., Konstantinova, T. S., Kopatskaya, E. N., Koptelova, E., Kurtanidze, O. M., Lähteenmäki, A., Lamerato, A., Larionov, V. M., Larionova, E. G., Larionova, L. V., Leto, P., Lindfors, E., Marscher, A. P., McHardy, I. M., Molina, S. N., Morozova, D. A., Nikolashvili, M. G., Nilsson, K., Reinthal, R., Roustazadeh, P., Sakamoto, T., Sigua, L. A., Sillanpää, A., Takalo, L., Tammi, J., Taylor, B., Tornikoski, M., Trigilio, C., Troitsky, I. S., and Umana, G. The structure and emission model of the relativistic jet in the quasar 3C 279 inferred from radio to high-energy γ-ray observations in 2008-2010. United States: N. p., 2012. Web. doi:10.1088/0004-637X/754/2/114.
Hayashida, M., Madejski, G. M., Nalewajko, K., Sikora, M., Wehrle, A. E., Ogle, P., Collmar, W., Larsson, S., Fukazawa, Y., Itoh, R., Chiang, J., Stawarz, Ł., Blandford, R. D., Richards, J. L., Max-Moerbeck, W., Readhead, A., Buehler, R., Cavazzuti, E., Ciprini, S., Gehrels, N., Reimer, A., Szostek, A., Tanaka, T., Tosti, G., Uchiyama, Y., Kawabata, K. S., Kino, M., Sakimoto, K., Sasada, M., Sato, S., Uemura, M., Yamanaka, M., Greiner, J., Kruehler, T., Rossi, A., Macquart, J. P., Bock, D. C. -J., Villata, M., Raiteri, C. M., Agudo, I., Aller, H. D., Aller, M. F., Arkharov, A. A., Bach, U., Benítez, E., Berdyugin, A., Blinov, D. A., Blumenthal, K., Böttcher, M., Buemi, C. S., Carosati, D., Chen, W. P., Paola, A. Di, Dolci, M., Efimova, N. V., Forné, E., Gómez, J. L., Gurwell, M. A., Heidt, J., Hiriart, D., Jordan, B., Jorstad, S. G., Joshi, M., Kimeridze, G., Konstantinova, T. S., Kopatskaya, E. N., Koptelova, E., Kurtanidze, O. M., Lähteenmäki, A., Lamerato, A., Larionov, V. M., Larionova, E. G., Larionova, L. V., Leto, P., Lindfors, E., Marscher, A. P., McHardy, I. M., Molina, S. N., Morozova, D. A., Nikolashvili, M. G., Nilsson, K., Reinthal, R., Roustazadeh, P., Sakamoto, T., Sigua, L. A., Sillanpää, A., Takalo, L., Tammi, J., Taylor, B., Tornikoski, M., Trigilio, C., Troitsky, I. S., & Umana, G. The structure and emission model of the relativistic jet in the quasar 3C 279 inferred from radio to high-energy γ-ray observations in 2008-2010. United States. https://doi.org/10.1088/0004-637X/754/2/114
Hayashida, M., Madejski, G. M., Nalewajko, K., Sikora, M., Wehrle, A. E., Ogle, P., Collmar, W., Larsson, S., Fukazawa, Y., Itoh, R., Chiang, J., Stawarz, Ł., Blandford, R. D., Richards, J. L., Max-Moerbeck, W., Readhead, A., Buehler, R., Cavazzuti, E., Ciprini, S., Gehrels, N., Reimer, A., Szostek, A., Tanaka, T., Tosti, G., Uchiyama, Y., Kawabata, K. S., Kino, M., Sakimoto, K., Sasada, M., Sato, S., Uemura, M., Yamanaka, M., Greiner, J., Kruehler, T., Rossi, A., Macquart, J. P., Bock, D. C. -J., Villata, M., Raiteri, C. M., Agudo, I., Aller, H. D., Aller, M. F., Arkharov, A. A., Bach, U., Benítez, E., Berdyugin, A., Blinov, D. A., Blumenthal, K., Böttcher, M., Buemi, C. S., Carosati, D., Chen, W. P., Paola, A. Di, Dolci, M., Efimova, N. V., Forné, E., Gómez, J. L., Gurwell, M. A., Heidt, J., Hiriart, D., Jordan, B., Jorstad, S. G., Joshi, M., Kimeridze, G., Konstantinova, T. S., Kopatskaya, E. N., Koptelova, E., Kurtanidze, O. M., Lähteenmäki, A., Lamerato, A., Larionov, V. M., Larionova, E. G., Larionova, L. V., Leto, P., Lindfors, E., Marscher, A. P., McHardy, I. M., Molina, S. N., Morozova, D. A., Nikolashvili, M. G., Nilsson, K., Reinthal, R., Roustazadeh, P., Sakamoto, T., Sigua, L. A., Sillanpää, A., Takalo, L., Tammi, J., Taylor, B., Tornikoski, M., Trigilio, C., Troitsky, I. S., and Umana, G. Mon . "The structure and emission model of the relativistic jet in the quasar 3C 279 inferred from radio to high-energy γ-ray observations in 2008-2010". United States. https://doi.org/10.1088/0004-637X/754/2/114. https://www.osti.gov/servlets/purl/1356717.
@article{osti_1356717,
title = {The structure and emission model of the relativistic jet in the quasar 3C 279 inferred from radio to high-energy γ-ray observations in 2008-2010},
author = {Hayashida, M. and Madejski, G. M. and Nalewajko, K. and Sikora, M. and Wehrle, A. E. and Ogle, P. and Collmar, W. and Larsson, S. and Fukazawa, Y. and Itoh, R. and Chiang, J. and Stawarz, Ł. and Blandford, R. D. and Richards, J. L. and Max-Moerbeck, W. and Readhead, A. and Buehler, R. and Cavazzuti, E. and Ciprini, S. and Gehrels, N. and Reimer, A. and Szostek, A. and Tanaka, T. and Tosti, G. and Uchiyama, Y. and Kawabata, K. S. and Kino, M. and Sakimoto, K. and Sasada, M. and Sato, S. and Uemura, M. and Yamanaka, M. and Greiner, J. and Kruehler, T. and Rossi, A. and Macquart, J. P. and Bock, D. C. -J. and Villata, M. and Raiteri, C. M. and Agudo, I. and Aller, H. D. and Aller, M. F. and Arkharov, A. A. and Bach, U. and Benítez, E. and Berdyugin, A. and Blinov, D. A. and Blumenthal, K. and Böttcher, M. and Buemi, C. S. and Carosati, D. and Chen, W. P. and Paola, A. Di and Dolci, M. and Efimova, N. V. and Forné, E. and Gómez, J. L. and Gurwell, M. A. and Heidt, J. and Hiriart, D. and Jordan, B. and Jorstad, S. G. and Joshi, M. and Kimeridze, G. and Konstantinova, T. S. and Kopatskaya, E. N. and Koptelova, E. and Kurtanidze, O. M. and Lähteenmäki, A. and Lamerato, A. and Larionov, V. M. and Larionova, E. G. and Larionova, L. V. and Leto, P. and Lindfors, E. and Marscher, A. P. and McHardy, I. M. and Molina, S. N. and Morozova, D. A. and Nikolashvili, M. G. and Nilsson, K. and Reinthal, R. and Roustazadeh, P. and Sakamoto, T. and Sigua, L. A. and Sillanpää, A. and Takalo, L. and Tammi, J. and Taylor, B. and Tornikoski, M. and Trigilio, C. and Troitsky, I. S. and Umana, G.},
abstractNote = {Here, we present time-resolved broadband observations of the quasar 3C 279 obtained from multi-wavelength campaigns conducted during the first two years of the Fermi Gamma-ray Space Telescope mission. And, while investigating the previously reported γ-ray/optical flare accompanied by a change in optical polarization, we found that the optical emission appears to be delayed with respect to the γ-ray emission by about 10 days. X-ray observations reveal a pair of "isolated" flares separated by ~90 days, with only weak γ-ray/optical counterparts. The spectral structure measured by Spitzer reveals a synchrotron component peaking in the mid-infrared band with a sharp break at the far-infrared band during the γ-ray flare, while the peak appears in the millimeter (mm)/submillimeter (sub-mm) band in the low state. Selected spectral energy distributions are fitted with leptonic models including Comptonization of external radiation produced in a dusty torus or the broad-line region. Furthermore, by adopting the interpretation of the polarization swing involving propagation of the emitting region along a curved trajectory, we can explain the evolution of the broadband spectra during the γ-ray flaring event by a shift of its location from ~1 pc to ~4 pc from the central black hole. On the other hand, if the γ-ray flare is generated instead at sub-pc distance from the central black hole, the far-infrared break can be explained by synchrotron self-absorption. We also model the low spectral state, dominated by the mm/sub-mm peaking synchrotron component, and suggest that the corresponding inverse-Compton component explains the steady X-ray emission.},
doi = {10.1088/0004-637X/754/2/114},
journal = {The Astrophysical Journal},
number = 2,
volume = 754,
place = {United States},
year = {Mon Jul 16 00:00:00 EDT 2012},
month = {Mon Jul 16 00:00:00 EDT 2012}
}

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Works referencing / citing this record:

Long-term multiwavelength studies of high-redshift blazar 0836+710
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Is there a non-stationary γ -ray emission zone 42 pc from the 3C 279 core?
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Resolving the High-Energy Universe with Strong Gravitational Lensing: the case of pks 1830–211
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Gamma-Ray Polarimetry: A New Window for the Nonthermal Universe
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A two-zone model for blazar emission: implications for TXS 0506+056 and the neutrino event IceCube-170922A
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Constraints on the emission region of 3C 279 during strong flares in 2014 and 2015 through VHE γ -ray observations with H.E.S.S.
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Minute-Timescale > 100 MeV $\gamma$-Ray Variability During the Giant Outburst of Quasar 3C 279 Observed by FERMI-LAT in 2015 June
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Compton Dominance and the Blazar Sequence
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Constraining the Location of Gamma-Ray Flares in Luminous Blazars
text, January 2014


Resolving the High Energy Universe with Strong Gravitational Lensing: The Case of PKS 1830-211
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A Steady-State Spectral Model For Electron Acceleration And Cooling In Blazar Jets: Application To 3C 279
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Multiwavelength Photometric and Spectropolarimetric Analysis of the FSRQ 3C 279
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New hard-TeV extreme blazars detected with the MAGIC telescopes
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Monitoring of the radio galaxy M87 during a low emission state from 2012 to 2015 with MAGIC
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