Multiwavelength Observations of the Galactic Black Hole Transient 4U 1543−47 during Outburst Decay: State Transitions and Jet Contribution

Kalemci, Emrah; Tomsick, John A.; Buxton, M.; Rothschild, R. E.; Pottschmidt, K.; Corbel, S.; Brocksopp, C.; Kaaret, Philip

doi:10.1086/427818

Cited by 108 publications

(179 citation statements)

References 61 publications

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“…Kalemci et al 2004;Yuan et al 2007;Yamaoka et al 2005). As in samples of AGN, they are seen to switch from a positive correlation to a negative correlation between Γ andṁ, and therefore from harder-when-brighter to softer-when-brighter behaviour, whenṁ Edd increases above a critical value,ṁcrit.…”

Section: Agn and Bhxrb State Analoguesmentioning

confidence: 75%

Long-term X-ray spectral variability in AGN from the Palomar sample observed bySwift

Connolly

McHardy

Skipper

et al. 2016

Mon. Not. R. Astron. Soc.

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We present X-ray spectral variability of 24 local active galactic nuclei (AGN) from the Palomar sample of nearby galaxies, as observed mainly by Swift. From hardness ratio measurements, we find that 18 AGN with low accretion rates show hardening with increasing count rate, converse to the softer-when-brighter behaviour normally observed in AGN with higher accretion rates. Two AGN show softening with increasing count rate, two show more complex behaviour, and two do not show any simple relationship.Sufficient data were available for the spectra of 13 AGN to be summed in fluxbins. In 9 of these sources, correlated luminosity-dependent changes in the photon index (Γ) of a power-law component are found to be the main cause of hardness variability. For 6 objects, with a low accretion rate as a fraction of the Eddington rate (ṁ Edd ), Γ is anticorrelated withṁ Edd , i.e. 'harder-when-brighter' behaviour is observed. The 3 higher-ṁ Edd -rate objects show a positive correlation between Γ anḋ m Edd . This transition from harder-when-brighter at lowṁ Edd to softer-when-brighter at highṁ Edd can be explained by a change in the dominant source of seed-photons for X-ray emission from cyclo-synchrotron emission from the Comptonising corona itself to thermal seed-photons from the accretion disc. This transition is also seen in the 'hard state' of black hole X-ray binaries (BHXRBs). The results support the idea that LINERs are analogues of BHXRBs in the hard state and that Seyferts are analogues of BHXRBs in either the high-accretion-rate end of the hard state or in the hard-intermediate state.

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Section: Agn and Bhxrb State Analoguesmentioning

confidence: 75%

Long-term X-ray spectral variability in AGN from the Palomar sample observed bySwift

Connolly

McHardy

Skipper

et al. 2016

Mon. Not. R. Astron. Soc.

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“…The X-ray photon index and the flux are taken from RXTE observations (Kalemci et al 2005, with the same spectral fitting model as that adopted for GX 339-4), and M BH = 9.4 M ⊙ and d = 7.5 kpc are from Park et al (2004).…”

Section: The Bhb Samplementioning

confidence: 99%

Correlation between the photon index and X-ray luminosity of black hole X-ray binaries and active galactic nuclei: observations and interpretation

Yang

Xie

Yuan

et al. 2014

Monthly Notices of the Royal Astronomical Society

121

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We investigate the observed correlation between the 2-10 keV X-ray luminosity (in unit of the Eddington luminosity; l X ≡ L X /L Edd ) and the photon index (Γ) of the X-ray spectrum for both black hole X-ray binaries (BHBs) and active galactic nuclei (AGNs). We construct a large sample, with 10 −9 < ∼ l X < ∼ 10 −1 . We find that Γ is positively and negatively correlated with l X when l X > ∼ 10 −3 and 10 −6.5 < ∼ l X < ∼ 10 −3 respectively, while Γ is nearly a constant when l X < ∼ 10 −6.5 . We explain the above correlation in the framework of a coupled hot accretion flow -jet model. The radio emission always come from the jet while the X-ray emission comes from the accretion flow and jet when l X is above and below 10 −6.5 , respectively. More specifically, we assume that with the increase of mass accretion rate, the hot accretion flow develops into a clumpy and further a disc -corona two-phase structure because of thermal instability. We argue that such kind of two-phase accretion flow can explain the observed positive correlation.

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“…However, the cause of the softening remains unclear, largely because observations with sufficient sensitivity and cadence to track the photon index as it approaches, reaches, and eventually saturates to G » 2.1 are scarce (see, e.g., Kalemci et al 2005;Homan et al 2013 for examples of some of the best covered decays so far).…”

Section: Introductionmentioning

confidence: 99%

The 2015 Decay of the Black Hole X-Ray Binary V404 Cygni: Robust Disk-Jet Coupling and a Sharp Transition Into Quiescence

Plotkin

Miller-Jones

Gallo

et al. 2017

ApJ

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We present simultaneous X-ray and radio observations of the black hole X-ray binary V404 Cygni at the end of its 2015 outburst. From 2015 July 11-August 5, we monitored V404 Cygni with Chandra, Swift, and NuSTAR in the X-ray, and with the Karl G. Jansky Very Large Array and the Very Long Baseline Array in the radio, spanning a range of luminosities that were poorly covered during its previous outburst in 1989 (our 2015 campaign covers10 erg s 33 X 34 1 ). During our 2015 campaign, the X-ray spectrum evolved rapidly from a hard photon index of). We argue that V404 Cygni reaching G » 2 marks the beginning of the quiescent spectral state, which occurs at a factor of ≈3-4 higher X-ray luminosity than the average pre-outburst luminosity of »´-8 10 erg s 32 1. V404 Cygni falls along the same radio/X-ray luminosity correlation that it followed during its previous outburst in 1989, implying a robust disk-jet coupling. We exclude the possibility that a synchrotron-cooled jet dominates the X-ray emission in quiescence, leaving synchrotron self-Compton from either a hot accretion flow or from a radiatively cooled jet as the most likely sources of X-ray radiation, and/or particle acceleration along the jet becoming less efficient in quiescence. Finally, we present the first indications of correlated radio and X-ray variability on minute timescales in quiescence, tentatively measuring the radio emission to lag the X-ray by  15 4 minute, suggestive of X-ray variations propagating down a jet with alength of<3.0 au.

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Multiwavelength Observations of the Galactic Black Hole Transient 4U 1543−47 during Outburst Decay: State Transitions and Jet Contribution

Cited by 108 publications

References 61 publications

Long-term X-ray spectral variability in AGN from the Palomar sample observed bySwift

Long-term X-ray spectral variability in AGN from the Palomar sample observed bySwift

Correlation between the photon index and X-ray luminosity of black hole X-ray binaries and active galactic nuclei: observations and interpretation

The 2015 Decay of the Black Hole X-Ray Binary V404 Cygni: Robust Disk-Jet Coupling and a Sharp Transition Into Quiescence

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