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NuSTAR and multifrequency study of the two high-redshift blazars S5 0836+710 and PKS 2149-306

Tagliaferri, G. and Ghisellini, G. and Perri, M. and Hayashida, M. and Baloković, M. and Covino, S. and Giommi, P. and Madejski, G. M. and Puccetti, S. and Sbarrato, T. and Boggs, S. E. and Chiang, J. and Christensen, F. E. and Craig, W. W. and Hailey, C. J. and Harrison, F. A. and Stern, D. and Zhang, W. W. (2015) NuSTAR and multifrequency study of the two high-redshift blazars S5 0836+710 and PKS 2149-306. Astrophysical Journal, 807 (2). Art. No. 167. ISSN 0004-637X. https://resolver.caltech.edu/CaltechAUTHORS:20150323-163935434

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Abstract

Powerful blazars are flat-spectrum radio quasars whose emission is dominated by a Compton component peaking between a few hundred keV and a few hundred MeV. We observed two bright blazars, PKS 2149–306 at redshift z = 2.345 and S5 0836+710 at z = 2.172, in the hard X-ray band with the Nuclear Spectroscopic Telescope Array satellite. Simultaneous soft-X-rays and UV–optical observations were performed with the Swift satellite, while near-infrared (near-IR) data were obtained with the Rapid Eye Mount telescope. To study their variability, we repeated these observations for both sources on a timescale of a few months. While no fast variability was detected during a single observation, both sources were variable in the X-ray band, up to 50%, between the two observations, with larger variability at higher energies. No variability was detected in the optical/NIR band. These data, together with Fermi-Large Area Telescope, Wide-field Infrared Survey Explorer, and other literature data, are then used to study the overall spectral energy distributions (SEDs) of these blazars. Although the jet nonthermal emission dominates the SED, it leaves the UV band unhidden, allowing us to detect the thermal emission of the disk and to estimate the black hole mass. The nonthermal emission is well reproduced by a one-zone leptonic model by the synchrotron, self-Compton, and external Compton processes. Our data are better reproduced if we assume that the location of the dissipation region of the jet, R_(diss), is in between the torus and the broad-line region. The observed variability is explained by changing a minimum number of model parameters by a very small amount.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://arxiv.org/abs/1503.04848arXivDiscussion Paper
http://dx.doi.org/10.1088/0004-637X/807/2/167DOIArticle
http://iopscience.iop.org/0004-637X/807/2/167/PublisherArticle
ORCID:
AuthorORCID
Puccetti, S.0000-0002-2734-7835
Boggs, S. E.0000-0001-9567-4224
Harrison, F. A.0000-0003-2992-8024
Stern, D.0000-0003-2686-9241
Additional Information:© 2015 American Astronomical Society. Received 2015 March 4; accepted 2015 May 18; published 2015 July 9. We acknowledge financial support from the ASI-INAF grant I/037/12/0. This work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by NASA. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. We also thank the Swift team for quickly approving and executing the requested ToO observations. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (Caltech, USA). The Fermi LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariat a l’Energie Atomique and the Centre National de la Recherche Scientifique / Institut National de Physique Nucleaire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK) and Japan Aerospace Exploration Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish Research Council and the Swedish National Space Board in Sweden. Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d’Etudes Spatiales in France. Part of this work is based on archival data, software or on-line services provided by the ASI Data Center (ASDC).
Group:NuSTAR, Space Radiation Laboratory
Funders:
Funding AgencyGrant Number
Agenzia Spaziale Italiana (ASI)I/037/12/0
NASANNG08FD60C
Istituto Nazionale di Astrofisica (INAF)UNSPECIFIED
Department of Energy (DOE)UNSPECIFIED
Commissariat à l’Energie Atomique (CEA)UNSPECIFIED
Institut National de Physique Nucleaire et de Physique des ParticulesUNSPECIFIED
Centre National de la Recherche Scientifique (CNRS)UNSPECIFIED
NASA/JPL/CaltechUNSPECIFIED
Ministry of Education, Culture, Sports, Science and Technology (MEXT)UNSPECIFIED
High Energy Accelerator Research Organization (KEK)UNSPECIFIED
Japan Aerospace Exploration Agency (JAXA)UNSPECIFIED
K. A. Wallenberg FoundationUNSPECIFIED
Swedish Research Council UNSPECIFIED
Swedish National Space Board (SNSB)UNSPECIFIED
Centre National d'Études Spatiales (CNES)UNSPECIFIED
Non-Subject Keywords:galaxies: active, quasars: general, X-rays: general, blazar: individual: PKS 2149–306, S5 0836+710
Other Numbering System:
Other Numbering System NameOther Numbering System ID
Space Radiation Laboratory2015-53
Issue or Number:2
Record Number:CaltechAUTHORS:20150323-163935434
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20150323-163935434
Official Citation:NuSTAR and Multifrequency Study of the Two High-redshift Blazars S5 0836+710 and PKS 2149–306 G. Tagliaferri et al. 2015 ApJ 807 167
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:55996
Collection:CaltechAUTHORS
Deposited By: Joy Painter
Deposited On:24 Mar 2015 16:14
Last Modified:03 Oct 2019 08:10

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