The variable iron K emission line in MCG—6-30-15

Iwasawa, K.; Fabian, A. C.; Reynolds, C. S.; Nandra, K.; Otani, Chiko; Inoue, Hajime; Hayashida, Kentaro; Brandt, W. N.; Dotani, Tadayasu; Kunieda, H.; Matsuoka, M.; Tanaka, Yasuo

doi:10.1093/mnras/282.3.1038

Cited by 291 publications

(382 citation statements)

References 20 publications

(47 reference statements)

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“…As is common with type-1 AGN, the X-ray flux of this AGN varied rapidly as a function of time. Via a detailed analysis of this and subsequent ASCA observations, Kazushi Iwasawa found that the iron line flux and profile also undergoes dramatic changes with time [207,208]. The detailed iron line changes are complex and defy simple characterization (see Fig.…”

Section: The First Detection Of a Relativistic Accretion Diskmentioning

confidence: 95%

Fluorescent iron lines as a probe of astrophysical black hole systems

2003

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Section: The First Detection Of a Relativistic Accretion Diskmentioning

confidence: 95%

Fluorescent iron lines as a probe of astrophysical black hole systems

2003

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“…A long ASCA observation of this source had caught its transition to the so-called "Deep Minimum State" in which Iwasawa et al (1996) noticed that the iron line was too broadened and redshifted to be explained by a non-rotating black hole. Subsequent modeling of this line profile by Dabrowski et al (1997) concluded that a > 0.95 under the assumption that the irradiation profile of the reflection follows a Novikov-Thorne profile.…”

Section: Early Historymentioning

confidence: 99%

Measuring Black Hole Spin Using X-Ray Reflection Spectroscopy

Reynolds¹

2013

The Physics of Accretion Onto Black Holes

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I review the current status of X-ray reflection (a.k.a. broad iron line) based black hole spin measurements. This is a powerful technique that allows us to measure robust black hole spins across the mass range, from the stellar-mass black holes in X-ray binaries to the supermassive black holes in active galactic nuclei. After describing the basic assumptions of this approach, I lay out the detailed methodology focusing on "best practices" that have been found necessary to obtain robust results. Reflecting my own biases, this review is slanted towards a discussion of supermassive black hole (SMBH) spin in active galactic nuclei (AGN). Pulling together all of the available XMM-Newton and Suzaku results from the literature that satisfy objective quality control criteria, it is clear that a large fraction of SMBHs are rapidlyspinning, although there are tentative hints of a more slowly spinning population at high (M > 5 × 10 7 M ⊙ ) and low (M < 2 × 10 6 M ⊙ ) mass. I also engage in a brief review of the spins of stellar-mass black holes in X-ray binaries. In general, reflection-based and continuum-fitting based spin measures are in agreement, although there remain two objects (GRO J1655-40 and 4U 1543-475) for which that is not true. I end this review by discussing the exciting frontier of relativistic reverberation, particularly the discovery of broad iron line reverberation in XMM-Newton data for the Seyfert galaxies NGC 4151, NGC 7314 and MCG-5-23-16. As well as confirming the basic paradigm of relativistic disk reflection, this detection of reverberation demonstrates that future large-area X-ray observatories such as LOFT will make tremendous progress in studies of strong gravity using relativistic reverberation in AGN.

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“…This is probably unrealistic: most black holes are expected to be spinning, some with angular momenta close to the unattainable extremal limit a ≡ J 2 /M 2 = a max = 1 in geometric units. There is some observational evidence for black holes in the stellar mass range with spins up to a = 0.94, and also of galactic black holes with similarly large spins [40,41].…”

Section: The Evaporation Time Of Large Black Holesmentioning

confidence: 99%

Black Hole Astrophysics in AdS Braneworlds

Emparan¹,

García-Bellido²,

Kaloper³

2003

J. High Energy Phys.

102

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We consider astrophysics of large black holes localized on the brane in the infinite RandallSundrum model. Using their description in terms of a conformal field theory (CFT) coupled to gravity, deduced in Ref.[1], we show that they undergo a period of rapid decay via Hawking radiation of CFT modes. For example, a black hole of mass few × M ⊙ would shed most of its mass in ∼ 10 4 − 10 5 years if the AdS radius is L ∼ 10 −1 mm, currently the upper bound from table-top experiments. Since this is within the mass range of X-ray binary systems containing a black hole, the evaporation enhanced by the hidden sector CFT modes could cause the disappearance of X-ray sources on the sky. This would be a striking signature of RS2 with a large AdS radius. Alternatively, for shorter AdS radii, the evaporation would be slower. In such cases, the persistence of X-ray binaries with black holes already implies an upper bound on the AdS radius of L < ∼ 10 −2 mm, an order of magnitude better than the bounds from table-top experiments. The observation of primordial black holes with a mass in the MACHO range M ∼ 0.1 − 0.5 M ⊙ and an age comparable to the age of the universe would further strengthen the bound on the AdS radius to L < ∼ few × 10 −6 mm. 1 roberto.emparan@cern.ch 2

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The variable iron K emission line in MCG—6-30-15

Cited by 291 publications

References 20 publications

Fluorescent iron lines as a probe of astrophysical black hole systems

Fluorescent iron lines as a probe of astrophysical black hole systems

Measuring Black Hole Spin Using X-Ray Reflection Spectroscopy

Black Hole Astrophysics in AdS Braneworlds

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