Energy-dependent variability and the origin of the soft X-ray excess in active galactic nuclei

Marek Gierliński (Lead / Corresponding author), Chris Done

Research output: Contribution to journalLetter

42 Citations (Scopus)
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Abstract

The origin of the soft excess seen in many active galactic nuclei (AGN) below ~1 keV is still an unsolved problem. It is unlikely to represent a true continuum component as its characteristic 'temperature' shows a remarkable constancy over a wide range of AGN luminosity and black hole mass. This instead favours an association with atomic processes, in particular with the increase in opacity between 0.7 and 2 keV associated with partially ionized O and Fe. The opacity jump can give rise to a soft excess through either reflection or transmission, and both scenarios can fit the spectra equally well as long as there is strong velocity shear to smear out the characteristic narrow atomic features. Here we use orthogonal constraints from the energy-dependent variability. The rms spectra seen in XMM-Newton AGN data often show a broad peak between 0.7 and 2 keV. We show that the absorption model can explain the data well if the ionization state of the smeared absorption responds to luminosity changes in the continuum.

Original languageEnglish
Number of pages5
JournalMonthly Notices of the Royal Astronomical Society: Letters
Volume371
Issue number1
DOIs
Publication statusPublished - 1 Sep 2006

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active galactic nuclei
opacity
constancy
luminosity
continuums
energy
smear
ionization
x rays
XMM-Newton telescope
newton
shear
temperature

Keywords

  • Accretion, accretion discs
  • Atomic processes
  • Galaxies: active
  • X-rays: galaxies

Cite this

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title = "Energy-dependent variability and the origin of the soft X-ray excess in active galactic nuclei",
abstract = "The origin of the soft excess seen in many active galactic nuclei (AGN) below ~1 keV is still an unsolved problem. It is unlikely to represent a true continuum component as its characteristic 'temperature' shows a remarkable constancy over a wide range of AGN luminosity and black hole mass. This instead favours an association with atomic processes, in particular with the increase in opacity between 0.7 and 2 keV associated with partially ionized O and Fe. The opacity jump can give rise to a soft excess through either reflection or transmission, and both scenarios can fit the spectra equally well as long as there is strong velocity shear to smear out the characteristic narrow atomic features. Here we use orthogonal constraints from the energy-dependent variability. The rms spectra seen in XMM-Newton AGN data often show a broad peak between 0.7 and 2 keV. We show that the absorption model can explain the data well if the ionization state of the smeared absorption responds to luminosity changes in the continuum.",
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T1 - Energy-dependent variability and the origin of the soft X-ray excess in active galactic nuclei

AU - Gierliński, Marek

AU - Done, Chris

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N2 - The origin of the soft excess seen in many active galactic nuclei (AGN) below ~1 keV is still an unsolved problem. It is unlikely to represent a true continuum component as its characteristic 'temperature' shows a remarkable constancy over a wide range of AGN luminosity and black hole mass. This instead favours an association with atomic processes, in particular with the increase in opacity between 0.7 and 2 keV associated with partially ionized O and Fe. The opacity jump can give rise to a soft excess through either reflection or transmission, and both scenarios can fit the spectra equally well as long as there is strong velocity shear to smear out the characteristic narrow atomic features. Here we use orthogonal constraints from the energy-dependent variability. The rms spectra seen in XMM-Newton AGN data often show a broad peak between 0.7 and 2 keV. We show that the absorption model can explain the data well if the ionization state of the smeared absorption responds to luminosity changes in the continuum.

AB - The origin of the soft excess seen in many active galactic nuclei (AGN) below ~1 keV is still an unsolved problem. It is unlikely to represent a true continuum component as its characteristic 'temperature' shows a remarkable constancy over a wide range of AGN luminosity and black hole mass. This instead favours an association with atomic processes, in particular with the increase in opacity between 0.7 and 2 keV associated with partially ionized O and Fe. The opacity jump can give rise to a soft excess through either reflection or transmission, and both scenarios can fit the spectra equally well as long as there is strong velocity shear to smear out the characteristic narrow atomic features. Here we use orthogonal constraints from the energy-dependent variability. The rms spectra seen in XMM-Newton AGN data often show a broad peak between 0.7 and 2 keV. We show that the absorption model can explain the data well if the ionization state of the smeared absorption responds to luminosity changes in the continuum.

KW - Accretion, accretion discs

KW - Atomic processes

KW - Galaxies: active

KW - X-rays: galaxies

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JO - Monthly Notices of the Royal Astronomical Society: Letters

JF - Monthly Notices of the Royal Astronomical Society: Letters

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