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The Accreting Black Hole Swift J1753.5-0127 from Radio to Hard X-Ray

Tomsick, John A. and Rahoui, Farid and Kolehmainen, Mari and Miller-Jones, James and Fuerst, Felix and Yamaoka, Kazutaka and Akitaya, Hiroshi and Corbel, Stéphane and Coriat, Mickael and Done, Chris and Gandhi, Poshak and Harrison, Fiona A. and Huang, Kuiyun and Kaaret, Philip and Kalemci, Emrah and Kanda, Yuka and Migliari, Simone and Miller, Jon M. and Moritani, Yuki and Stern, Daniel and Uemura, Makoto and Urata, Yuji (2015) The Accreting Black Hole Swift J1753.5-0127 from Radio to Hard X-Ray. Astrophysical Journal, 808 (1). Art. No. 85. ISSN 0004-637X. doi:10.1088/0004-637X/808/1/85.

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We report on multi-wavelength measurements of the accreting black hole Swift J1753.5–0127 in the hard state at low luminosity (L ∼ 2.7×10^(36) erg s^(−1) assuming a distance of d = 3 kpc) in 2014 April. The radio emission is optically thick synchrotron, presumably from a compact jet. We take advantage of the low extinction (E(B−V) = 0.45 from earlier work) and model the near-IR to UV emission with a multi-temperature disk model. Assuming a black hole mass of MBH = 5M⊙ and a system inclination of i = 40^◦, the fits imply an inner radius for the disk of R_(in)/R_g > 212 d3 (MBH/5M_⊙)^−1, where R_g is the gravitational radius of the black hole, and d_3 is the distance to the source in units of 3 kpc. The outer radius is R_(out)/R_g = 90,000 d_3 (MBH/5M_⊙)^(−1), which corresponds to 6.6×10^(10) d_3 cm, consistent with the expected size of the disk given previous measurements of the size of the companion’s Roche lobe. The 0.5–240 keV energy spectrum measured by Swift/XRT, Suzaku (XIS, PIN, and GSO), and NuSTAR is relatively well characterized by an absorbed power-law with a photon index of Γ = 1.722±0.003 (90% confidence error), but a significant improvement is seen when a second continuum component is added. Reflection is a possibility, but no iron line is detected, implying a low iron abundance. We are able to fit the entire (radio to 240 keV) spectral energy distribution (SED) with a multi-temperature disk component, a Comptonization component, and a broken power-law, representing the emission from the compact jet. The broken power-law cannot significantly contribute to the soft X-ray emission, and this may be related to why Swift J1753.5–0127 is an outlier in the radio/X-ray correlation. The broken power-law (i.e., the jet) might dominate above 20 keV, which would constrain the break frequency to be between 2.4×10^(10) Hz and 3.6×10^(12) Hz. Although the fits to the full SED do not include significant thermal emission in the X-ray band, previous observations have consistently seen such a component, and we find that there is evidence at the 3.1-σ level for a disk-blackbody component with a temperature of kTin = 150 +30/−20 eV and an inner radius of 5–14R_g. If this component is real, it might imply the presence of an inner optically thick accretion disk in addition to the strongly truncated (R_(in) > 212R_g) disk. We also perform X-ray timing analysis, and the power spectrum is dominated by a Lorentzian component with νmax = 0.110±0.003Hz and νmax = 0.16±0.04 Hz as measured by XIS and XRT, respectively.

Item Type:Article
Related URLs:
URLURL TypeDescription Paper
Tomsick, John A.0000-0001-5506-9855
Rahoui, Farid0000-0001-7655-4120
Fuerst, Felix0000-0003-0388-0560
Gandhi, Poshak0000-0003-3105-2615
Harrison, Fiona A.0000-0003-2992-8024
Kaaret, Philip0000-0002-3638-0637
Stern, Daniel0000-0003-2686-9241
Additional Information:© 2015 American Astronomical Society. Received 2015 April 29; accepted 2015 June 15; published 2015 July 22. We thank the referee for useful comments that helped to improve the manuscript. 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 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). The PS1 Surveys have been made possible through contributions of the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, Queen’s University Belfast, the Harvard-Smithsonian Center for Astrophysics, and the Las Cumbres Observatory Global Telescope Network, Incorporated, the National Central University of Taiwan, and the National Aeronautics and Space Administration under Grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate. JAT acknowledges partial support from NASA under Swift Guest Observer grants NNX13AJ81G and NNX14AC56G. SC acknowledges the financial support from the UnivEarthS Labex programme of Sorbonne Paris Cité (ANR-10-LABX-0023 and ANR-11-IDEX-0005-02), and from the CHAOS project ANR-12-BS05-0009 supported by the French Research National Agency. JMJ is supported by an Australian Research Council (ARC) Future Fellowship (FT140101082) and also acknowledges support from an ARC Discovery Grant. EK acknowledges support from TUBITAK BIDEB 2219 program. This work was supported by the Spanish Ministerio de Economá y Competitividad (MINECO) under grant AYA2013-47447-C3-1-P (SM).
Group:NuSTAR, Space Radiation Laboratory
Funding AgencyGrant Number
Agence Nationale pour la Recherche (ANR)ANR-10-LABX-0023
Agence Nationale pour la Recherche (ANR)ANR-11-IDEX-0005-02
Agence Nationale pour la Recherche (ANR)ANR-12-BS05-0009
Australian Research Council (ARC)FT140101082
Türkiye Bilimsel ve Teknolojik Araştırma Kurumu (TÜBİTAK)BIDEB 2219
Ministerio de Economá y Competitividad (MINECO)AYA2013-47447-C3-1-P
Subject Keywords:accretion, accretion disks – black hole physics – stars: individual (Swift J1753.5–0127) – X-rays: general – X-rays: stars
Other Numbering System:
Other Numbering System NameOther Numbering System ID
Space Radiation Laboratory2015-49
Issue or Number:1
Record Number:CaltechAUTHORS:20150802-075928230
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Official Citation: The Accreting Black Hole Swift J1753.5–0127 from Radio to Hard X-Ray John A. Tomsick et al. 2015 ApJ 808 85
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:59138
Deposited By: Joy Painter
Deposited On:06 Aug 2015 18:34
Last Modified:10 Nov 2021 22:15

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