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

Tomsick, J.A.; Rahoui, F.; Kolehmainen, M.; Miller-Jones, J.; Fürst, F.; Yamaoka, K.; Akitaya, H.; Corbel, S.; Coriat, M.; Done, C.; Gandhi, P.; Harrison, F.A.; Huang, K.; Kaaret, P.; Kalemci, E.; Kanda, Y.; Migliari, S.; Miller, J.M.; Moritani, Y.; Stern, D.; Uemura, M.; Urata, Y.

Abstract

We report on multiwavelength measurements of the accreting black hole Swift J1753.5–0127 in the hard state at low luminosity (L ~ 2.7 × 1036 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 multitemperature disk model. Assuming a black hole mass of MBH = 5 M⊙ and a system inclination of i = 40°, the fits imply an inner radius for the disk of Rin/Rg > 212d3(MBH/5 M⊙)−1, where Rg is the gravitational radius of the black hole and d3 is the distance to the source in units of 3 kpc. The outer radius is Rout/Rg=90,000 d3(MBH/5 M⊙)−1, which corresponds to 6.6 × 1010 d3 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/X-ray Telescope (XRT), Suzaku (XIS, PIN, and GSO), and Nuclear Spectroscopic Telescope Array 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 multitemperature 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 × 1010 and 3.6 × 1012 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 3.1σ level for a disk-blackbody component with a temperature of ${{kT}}_{\mathrm{in}}={150}_{-20}^{+30}$ eV and an inner radius of 5Rg–14Rg. If this component is real, it might imply the presence of an inner optically thick accretion disk in addition to the strongly truncated (Rin> 212Rg) disk. We also perform X-ray timing analysis, and the power spectrum is dominated by a Lorentzian component with νmax = 0.110 ± 0.003 Hz and νmax = 0.16 ± 0.04 Hz as measured by XIS and XRT, respectively.

Citation

Tomsick, J., Rahoui, F., Kolehmainen, M., Miller-Jones, J., Fürst, F., Yamaoka, K., …Urata, Y. (2015). The Accreting Black Hole Swift J1753.5-0127 from Radio to Hard X-Ray. Astrophysical Journal, 808(1), https://doi.org/10.1088/0004-637x/808/1/85

• Journal Article Type: Article
• Acceptance Date: Jun 15, 2015
• Online Publication Date: Jul 22, 2015
• Publication Date: Jul 22, 2015
• Deposit Date: Mar 16, 2016
• Publicly Available Date: Apr 8, 2016
• Journal: Astrophysical Journal
• Print ISSN: 0004-637X
• Electronic ISSN: 1538-4357
• Publisher: American Astronomical Society
• Peer Reviewed: Peer Reviewed
• Volume: 808
• Issue: 1
• DOI: https://doi.org/10.1088/0004-637x/808/1/85
• Public URL: https://durham-repository.worktribe.com/output/1416718