4.7 Article

A full characterization of the supermassive black hole in IRAS09149-6206

期刊

出版社

OXFORD UNIV PRESS
DOI: 10.1093/mnras/staa2961

关键词

black hole physics; galaxies: active; X-rays: individual (IRAS 09149-6206)

资金

  1. Science and Technology Facilities Council (STFC) via an Ernest Rutherford Fellowship
  2. STFC studentship
  3. NASA [80NSSC19K1020, 80NSSC19K0586]
  4. Alexander von Humboldt Foundation
  5. ASI-INAF [2017-14-H.0]
  6. EU Horizon 2020 Marie Sklodowska-Curie grant [664931]
  7. Fondecyt Iniciacion grant [11190831]
  8. STFC [ST/R000867/1]
  9. European Research Council under the European Union's Horizon 2020 research and innovation programme [834203]
  10. NASA
  11. ESA Member States
  12. STFC [ST/R000867/1, ST/S000623/1, ST/N004027/1] Funding Source: UKRI

向作者/读者索取更多资源

We present new broad-band X-ray observations of the type-I Seyfert galaxy IRAS 09149-6206, taken in 2018 with XMM-Newton, NuSTAR, and Swift. The source is highly complex, showing a classic 'warm' X-ray absorber, additional absorption from highly ionized iron, strong relativistic reflection from the innermost accretion disc and further reprocessing by more distant material. By combining X-ray timing and spectroscopy, we have been able to fully characterize the supermassive black hole in this system, constraining both its mass and - for the first time - its spin. The mass is primarily determined by X-ray timing constraints on the break frequency seen in the power spectrum, and is found to be log [M-BH/M-circle dot] = 8.0 +/- 0.6 (1s uncertainties). This is in good agreement with previous estimates based on the H alpha and H beta line widths, and implies that IRAS 09149-6206 is radiating at close to (but still below) its Eddington luminosity. The spin is constrained via detailed modelling of the relativistic reflection, and is found to be a* = 0.94(-0.07)(+0.02) (90 per cent confidence), adding IRAS 09149-6206 to the growing list of radio-quiet active galactic nuclei (AGNs) that host rapidly rotating black holes. The outflow velocities of the various absorption components are all relatively modest (upsilon(out) less than or similar to 0.03c), implying these are unlikely to drive significant galaxy-scale AGN feedback.

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