Broad iron L line and X-ray reverberation in 1H0707-495

By A. Zoghbi, A. C. Fabian, P. Uttley, G. Miniutti, L. Gallo, C. Reynolds, Jon M. Miller, G. Ponti. 2009

207 citations recorded by the source corpus.

A detailed analysis of a long XMM-Newton observation of the narrow-line type 1 Seyfert galaxy 1H0707-495 is presented, including spectral fitting, spectral variability and timing studies. The two main features in the spectrum are the drop at ?7?keV and a complex excess below 1?keV. These are well described by two broad, K and L, iron lines. Alternative models based on absorption, although they may fit the high-energy drop, cannot account for the 1?keV complexity and the spectrum as a whole. Spectral variability shows that the spectrum is composed of at least two components, which are interpreted as a power law dominating between 1-4?keV and a reflection component outside this range. The high count rate at the iron L energies has enabled us to measure a significant soft lag of ?30 s between 0.3-1 and 1-4?keV, meaning that the direct hard emission leads the reflected emissions. We interpret the lag as a reverberation signal originating within a few gravitational radii of the black hole.

View Paper: https://www.semanticscholar.org/paper/8a68626d96bbde13d66fa107f62b6f4d845ab2e3

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

1. J. E. McClintock
2. Ramesh Narayan
3. T. Dauser
4. J. Steiner
5. Cosimo Bambi
6. Lijun Gou
7. C. Reynolds
8. Ronald A. Remillard

Citations in the corpus

• The spin of the black hole microquasar XTE J1550−564 via the continuum-fitting and Fe-line methods (2010, methodology): “…stellar BHs (Blum et al. 2009; Miller et al. 2009b; Reis et al. 2009, 2011) and supermassive BHs (Brenneman & Reynolds 2006; Fabian et al. 2009; Miniutti et al. 2009; Schmoll et al. 2009; Zoghbi et al. 2010) have been reported using the Fe-line method with values ranging from a∗ ≈ 0 to a∗ > 0.98.”
• A global look at X-ray time lags in seyfert galaxies (2016, background): “X-ray reverberation lags were first robustly discovered in the source 1H 0707-495, which is one of the most highly variable and well-observed Seyfert galaxies in the XMM- ⋆ E-mail: ekara@astro.umd.edu Newton archive (Fabian et al. 2009; Zoghbi et al. 2010).”
• Suzaku observations of 'bare' active galactic nuclei (2012, methodology): “…this source is well documented as having a deep, sharp drop above ∼7 keV (Boller et al. 2002; Fabian et al. 2004, 2009, 2012b; Gallo et al. 2004; Zoghbi et al. 2010), which is not detected owing to the poor data quality, leading to the same problems in determining the iron abundance, disc…”
• Discovery of a relation between black hole mass and soft X-ray time lags in active galactic nuclei (2011, methodology): “…significant detection of a soft/negative lag in AGN light curves was reported in the narrow line Seyfert 1 galaxy 1H 0707−495 (Fabian et al. 2009; Zoghbi et al. 2010), and interpreted as the signature of relativistic reflection which ‘reverberates’ in response to continuum changes after a time…”
• Understanding X‐ray reflection emissivity profiles in AGN: locating the X‐ray source (2012, background): “Fabian et al. (2009) and Zoghbi et al. (2010) report reverberation time lags of around 30 s where variability in the reflection dominated component of the spectrum is seen to respond to that in the power law continuum after a time lag due to the finite light travel time from the primary Xray source…”
• X-ray reverberation around accreting black holes (2014, background): “At low frequencies, below ∼ 1 Hz, the disc variations lead the powerlaw variations, by tenths of a second, consistent with fluctuations propagating through the disc to the inner corona on a viscous time-scale, requiring that the disc, if thin (H/R 0.1), extends to relatively small radii, within ∼ ”
• Measuring Black Hole Spin Using X-Ray Reflection Spectroscopy (2013, background): “Fabian et al. (2009) discovered that, at intermediate timescales, the soft-excess lags the 2–4 keV continuum band by ∼ 30 s (also see detailed follow-up work by Zoghbi et al. 2010).”
• IMPROVED REFLECTION MODELS OF BLACK HOLE ACCRETION DISKS: TREATING THE ANGULAR DISTRIBUTION OF X-RAYS (2013, background): “However, further studies (e.g., timing measurements; see Zoghbi et al. 2010; Kara et al. 2013a,b), are required to accurately determine the illumination profile and the physical origin of the primary source itself.”
• Irradiation of an accretion disc by a jet: general properties and implications for spin measurements of black holes (2013, methodology): “Recent work has been applying a more selfconsistent approach by including models for the relativistic distortion of the full reflection spectrum during the data analysis (see, e.g., Zoghbi et al. 2010; Duro et al. 2011; Fabian et al.2012b; Dauser et al. 2012).”
• Relativistic iron K X-ray reverberation in NGC 4151 (2011, background): “Short time delays have first been seen in the Narrow Line Seyfert 1 galaxy 1H0707-495 (Fabian et al. 2009; Zoghbi et al. 2010).”
• THE SPIN OF THE SUPERMASSIVE BLACK HOLE IN NGC 3783 (2011, unknown): “4 + 5654, Miniutti et al. 2009; 1H0707–495, Zoghbi et al. 2010; Mrk 79, Gallo et al. 2011; Mrk 335 and NGC 7469, Patrick et al. 2011; see Table 2).”