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NuSTAR, Swift, and GROND observations of the flaring MeV blazar: PMN J0641−0320

Ajello, M. and Ghisellini, G. and Paliya, V. S. and Kocevski, D. and Tagliaferri, G. and Madejski, G. and Rau, A. and Schady, P. and Greiner, J. and Massaro, F. and Baloković, M. and Bühler, R. and Giomi, M. and Marcotulli, L. and D'Ammando, F. and Stern, D. and Boggs, S. E. and Christensen, F. E. and Craig, W. W. and Hailey, C. J. and Harrison, F. A. and Zhang, W. W. (2016) NuSTAR, Swift, and GROND observations of the flaring MeV blazar: PMN J0641−0320. Astrophysical Journal, 826 (1). Art. No. 76. ISSN 0004-637X. doi:10.3847/0004-637X/826/1/76.

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MeV blazars are a sub-population of the blazar family, exhibiting larger-than-average jet powers, accretion luminosities, and black hole masses. Because of their extremely hard X-ray continua, these objects are best studied in the X-ray domain. Here, we report on the discovery by the Fermi Large Area Telescope and subsequent follow-up observations with NuSTAR, Swift, and GROND of a new member of the MeV blazar family: PMN J0641−0320. Our optical spectroscopy provides confirmation that this is a flat-spectrum radio quasar located at a redshift of z = 1.196. Its very hard NuSTAR spectrum (power-law photon index of ~1 up to ~80 keV) indicates that the emission is produced via inverse Compton scattering off of photons coming from outside the jet. The overall spectral energy distribution of PMN J0641−0320 is typical of powerful blazars and, using a simple one-zone leptonic emission model, we infer that the emission region is located either inside the broad line region or within the dusty torus.

Item Type:Article
Related URLs:
URLURL TypeDescription Paper
Ajello, M.0000-0002-6584-1703
Paliya, V. S.0000-0001-7774-5308
Rau, A.0000-0001-5990-6243
Baloković, M.0000-0003-0476-6647
Stern, D.0000-0003-2686-9241
Boggs, S. E.0000-0001-9567-4224
Christensen, F. E.0000-0001-5679-1946
Harrison, F. A.0000-0003-2992-8024
Zhang, W. W.0000-0002-1426-9698
Additional Information:© 2016 The American Astronomical Society. Received 2016 February 20; revised 2016 April 21; accepted 2016 April 22; published 2016 July 22. We thank the anonymous referee for useful comments. M.A. acknowledges generous support from NASA grant NNH09ZDA001N. M.B. acknowledges support from the International Fulbright Science and Technology Award and from NASA Headquarters under the NASA Earth and Space Science Fellowship Program, grant NNX14AQ07H. 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 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 à l'Energie Atomique and the Centre National de la Recherche Scientifique/Institut National de Physique Nucléaire 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'Études Spatiales in France. This NuSTAR 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 the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software, and Calibration teams for support with the execution and analysis of these 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 (USA). Part of this work is based on archival data, software, or on-line services provided by the ASI Data Center (ASDC). This research has made use of the XRT Data Analysis Software (XRTDAS). Part of the funding for GROND (both hardware and personnel) was generously granted by the Leibniz-Prize to G. Hasinger (DFG grant HA 1850/28-1). Facilities: Fermi/LAT, NuSTAR, Swift, GROND, Keck.
Group:NuSTAR, Space Radiation Laboratory
Funding AgencyGrant Number
Fulbright FoundationUNSPECIFIED
NASA Earth and Space Science FellowshipNNX14AQ07H
Department of Energy (DOE)UNSPECIFIED
Commissariat a l'Energie Atomique (CEA)UNSPECIFIED
Centre National de la Recherche Scientifique (CNRS)UNSPECIFIED
Institut National de Physique Nucleaire et de Physique des Particules (IN2P3)UNSPECIFIED
Agenzia Spaziale Italiana (ASI)UNSPECIFIED
Istituto Nazionale di Fisica Nucleare (INFN)UNSPECIFIED
Ministry of Education, Culture, Sports, Science and Technology (MEXT)UNSPECIFIED
High Energy Accelerator Research Organization (KEK)UNSPECIFIED
Japan Aerospace Exploration Agency (JAXA)UNSPECIFIED
Knut and Alice Wallenberg FoundationUNSPECIFIED
Swedish Research CouncilUNSPECIFIED
Swedish National Space Board (SNSB)UNSPECIFIED
Istituto Nazionale di Astrofisica (INAF)UNSPECIFIED
Centre National d'Études Spatiales (CNES)UNSPECIFIED
Deutsche Forschungsgemeinschaft (DFG)HA 1850/28-1
Subject Keywords:galaxies: active – quasars: general – quasars: individual (PMN J0641–0320) – X-rays: general
Other Numbering System:
Other Numbering System NameOther Numbering System ID
Space Radiation Laboratory2016-20
Issue or Number:1
Record Number:CaltechAUTHORS:20160318-090815693
Persistent URL:
Official Citation:M. Ajello et al 2016 ApJ 826 76
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:65473
Deposited By: Ruth Sustaita
Deposited On:18 Mar 2016 17:27
Last Modified:10 Nov 2021 23:46

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