The Lx–Luv–Lradio relation and corona–disc–jet connection in optically selected radio-loud quasars

Author:

Zhu (朱世甫) S F12ORCID,Brandt W N123,Luo (罗斌) B4,Wu (武剑锋) Jianfeng5,Xue (薛永泉) Y Q67,Yang (杨光) G89ORCID

Affiliation:

1. Department of Astronomy & Astrophysics, The Pennsylvania State University, University Park, PA 16802, USA

2. Institute for Gravitation and the Cosmos, The Pennsylvania State University, University Park, PA 16802, USA

3. Department of Physics, 104 Davey Lab, The Pennsylvania State University, University Park, PA 16802, USA

4. School of Astronomy and Space Science, Nanjing University, Nanjing, Jiangsu 210046, China

5. Department of Astronomy, Xiamen University, Xiamen, Fujian 361005, China

6. CAS Key Laboratory for Research in Galaxies and Cosmology, Department of Astronomy, University of Science and Technology of China, Hefei 230026, China

7. School of Astronomy and Space Sciences, University of Science and Technology of China, Hefei 230026, China

8. Department of Physics and Astronomy, Texas A&M University, College Station, TX 77843-4242, USA

9. George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy, Texas A&M University, College Station, TX 77843-4242, USA

Abstract

ABSTRACT Radio-loud quasars (RLQs) are more X-ray luminous than predicted by the X-ray–optical/UV relation (i.e. $L_\mathrm{x}\propto L_\mathrm{uv}^\gamma$) for radio-quiet quasars (RQQs). The excess X-ray emission depends on the radio-loudness parameter (R) and radio spectral slope (αr). We construct a uniform sample of 729 optically selected RLQs with high fractions of X-ray detections and αr measurements. We find that steep-spectrum radio quasars (SSRQs; αr ≤ −0.5) follow a quantitatively similar $L_\mathrm{x}\propto L_\mathrm{uv}^{\gamma }$ relation as that for RQQs, suggesting a common coronal origin for the X-ray emission of both SSRQs and RQQs. However, the corresponding intercept of SSRQs is larger than that for RQQs and increases with R, suggesting a connection between the radio jets and the configuration of the accretion flow. Flat-spectrum radio quasars (FSRQs; αr > −0.5) are generally more X-ray luminous than SSRQs at given Luv and R, likely involving more physical processes. The emergent picture is different from that commonly assumed where the excess X-ray emission of RLQs is attributed to the jets. We thus perform model selection to compare critically these different interpretations, which prefers the coronal scenario with a corona–jet connection. A distinct jet component is likely important for only a small portion of FSRQs. The corona–jet, disc–corona, and disc–jet connections of RLQs are likely driven by independent physical processes. Furthermore, the corona–jet connection implies that small-scale processes in the vicinity of supermassive black holes, probably associated with the magnetic flux/topology instead of black hole spin, are controlling the radio-loudness of quasars.

Funder

NASA

National Natural Science Foundation of China

National Key R&D Program of China

ESA

Publisher

Oxford University Press (OUP)

Subject

Space and Planetary Science,Astronomy and Astrophysics

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