Bright radio emission from an ultraluminous stellar-mass microquasar in M 31

Middleton, Matthew; Miller-Jones, J. C. A.; Markoff, Sera; Fender, R. P.; Henze, M.; Hurley‐Walker, N.; Scaife, Anna M. M.; Roberts, T. P.; Walton, D. J.; Carpenter, John M.; Macquart, Jean–Pierre; Bower, Geoffrey C.; Gurwell, M. A.; Pietsch, W.; Haberl, F.; Harris, J.; Daniel, M. K.; Miah, J. A.; Done, Chris; Morgan, John S.; Dickinson, H. J.; Charles, P. A.; Burwitz, V.; Valle, M. Della; Freyberg, M. J.; Greiner, J.; Hernanz, M.; Hartmann, D. H.; Hatzidimitriou, D.; Riffeser, A.; Sala, G.; Seitz, S.; Reig, P.; Rau, A.; Orio, Marina; Titterington, D.; Grainge, Keith

doi:10.1038/nature11697

Cited by 118 publications

(128 citation statements)

References 37 publications

(14 reference statements)

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“…This is further confirmed by the detection of a classic sub-Eddington thermal dominant (high/soft) state when the X-ray luminosity drops below ∼10 39 erg s −1 . Then, using the constraints on the Eddington luminosity, Middleton et al (2013) estimate a black hole mass of ∼10 M . Also, Liu et al (2013) confirm a probable Wolf-Rayet companion star to a supersoft ULX in M101.…”

Section: Introductionmentioning

confidence: 99%

Irradiated, colour-temperature-corrected accretion discs in ultraluminous X-ray sources

Sutton¹,

Done²,

Roberts³

2014

Monthly Notices of the Royal Astronomical Society

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Although attempts have been made to constrain the stellar types of optical counterparts to ULXs, the detection of optical variability instead suggests that they may be dominated by reprocessed emission from X-rays which irradiate the outer accretion disc. Here, we report results from a combined X-ray and optical spectral study of a sample of ULXs, which were selected for having broadened disc-like X-ray spectra, and known optical counterparts. We simultaneously fit optical and X-ray data from ULXs with a new spectral model of emission from an irradiated, colour-temperaturecorrected accretion disc around a black hole, with a central Comptonising corona. We find that the ULXs require reprocessing fractions of ∼ 10 −3 , which is similar to sub-Eddington thermal dominant state BHBs, but less than has been reported for ULXs with soft ultraluminous X-ray spectra. We suggest that the reprocessing fraction may be due to the opposing effects of self-shielding in a geometrically thick super-critical accretion disc, and reflection from far above the central black hole by optically thin material ejected in a natal super-Eddington wind. Then, the higher reprocessing fractions reported for ULXs with wind-dominated X-ray spectra may be due to enhanced scattering onto the outer disc via the stronger wind in these objects. Alternatively, the accretion discs in these ULXs may not be particularly geometrically thick, rather they may be similar in this regard to the thermal dominant state BHBs.

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Section: Introductionmentioning

confidence: 99%

Irradiated, colour-temperature-corrected accretion discs in ultraluminous X-ray sources

Sutton¹,

Done²,

Roberts³

2014

Monthly Notices of the Royal Astronomical Society

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“…The identification of a long super-Eddington accretion phase in 3XMM J150052.0+015452 was strongly supported by the generally quasi-soft X-ray spectra, whose characteristic temperatures are too high to be explained by the standard thermal thin disk below the Eddington limit, but are consistent with Comptonized emission from a low-temperature optical thick corona. Similar spectra are commonly seen in ultraluminous X-ray sources (ULXs) (Gladstone et al 2009;Lin et al 2013b;Middleton et al 2013), most of which are believed to be super-Eddington accreting stellar-mass BHs, except that 3XMM J150052.0+015452 had orders of magnitude higher luminosities.…”

Section: The Tde Explanationmentioning

confidence: 76%

Large decay of X-ray flux in 2XMM J123103.2+110648: evidence for a tidal disruption event

Lin

Godet

et al. 2017

Monthly Notices of the Royal Astronomical Society

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The X-ray source 2XMM J123103.2+110648 was previously found to show pure thermal X-ray spectra and a ∼3.8 hr periodicity in three XMM-Newton X-ray observations in [2003][2004][2005], and the optical spectrum of the host galaxy suggested it as a type 2 active galactic nucleus candidate. We have obtained new X-ray observations of the source, with Swift and Chandra in 2013-2016, in order to shed new light on its nature based on its long-term evolution property. We found that the source could be in an X-ray outburst, with the X-ray flux decreasing by an order of magnitude in the Swift and Chandra observations, compared with the XMM-Newton observations ten years ago. There seemed to be significant spectral softening associated with the drop of Xray flux (disk temperature kT ∼ 0.16-0.2 keV in XMM-Newton observations versus kT ∼ 0.09 ± 0.02 keV in the Chandra observation). Therefore the Swift and Chandra follow-up observations support our previous suggestion that the source could be a tidal disruption event (TDE), though it seems to evolve slower than most of the other TDE candidates. The apparent long duration of this event could be due to the presence of a long super-Eddington accretion phase and/or slow circularization.

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“…On the other hand, as for the outbursts in the low mass X-ray binary (LMXB) transients, no saturation of the peak luminosity, up to the Eddington luminosity, is seen in the relation between the X-ray outburst peak luminosity and the orbital period in the Galactic transients (Wu et al 2010). These empirical relations suggested that some stellar mass compact objects can turn into ultra-luminous X-ray sources during brighter outbursts of similar duration or shorter outbursts (Yu & Yan 2009), which has been indeed observed (Middleton et al 2013). The correlation between the peak power of episodic jet and the corresponding peak luminosity of the soft state in Galactic sources suggests that the investigation of the relation between the episodic jet power and the peak luminosity of the soft state in transient ULXs would tell us about the nature of the ULXs as compared with the Galactic black hole transients; whether ULXs contains intermediate mass black holes or just extreme versions of the Galactic microquasars.…”

Section: Extension To Ultra-luminous X-ray Sources In Nearby Galaxiesmentioning

confidence: 88%

“…In order to address this question, we have investigated two transient ULXs in which radio emission from episodic jet has been detected during their outbursts. One of the ULXs is XMMU J004243.6+412519, which was first detected by XMM-Newton on 15 January 2012 (Henze et al 2012) as an ultra-luminous stellarmass microquasar (∼ 10 M⊙, see Middleton et al 2013) in M31, at a distance of only 0.78 Mpc away from us. Bright radio emission was observed from this source with similar behaviour to those Galactic black hole binaries (Middleton et al 2013).…”

Section: Extension To Ultra-luminous X-ray Sources In Nearby Galaxiesmentioning

confidence: 99%

“…One of the ULXs is XMMU J004243.6+412519, which was first detected by XMM-Newton on 15 January 2012 (Henze et al 2012) as an ultra-luminous stellarmass microquasar (∼ 10 M⊙, see Middleton et al 2013) in M31, at a distance of only 0.78 Mpc away from us. Bright radio emission was observed from this source with similar behaviour to those Galactic black hole binaries (Middleton et al 2013). The peak radio flux of the first VLA observation ever measured was around 0.5 mJy at 5.26 GHz.…”

Section: Extension To Ultra-luminous X-ray Sources In Nearby Galaxiesmentioning

confidence: 99%

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Discovery of the correlation between peak episodic jet power and X-ray peak luminosity of the soft state in black hole transients

Zhang¹,

Yu²

2015

Monthly Notices of the Royal Astronomical Society

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Episodic jets are usually observed in the intermediate state of black hole transients during their X-ray outbursts. Here we report the discovery of a strong positive correlation between the peak radio power of the episodic jet P jet and the corresponding peak X-ray luminosity L x of the soft state (in Eddington units) in a complete sample of the outbursts of black hole transients observed during the RXTE era of which data are available, which follows the relation log P jet = (2.2 ± 0.3) + (1.6 ± 0.2) × log L x . The transient ultra-luminous X-ray source in M31 and HLX-1 in EXO 243-49 fall on the relation if they contain stellar mass black hole and either stellar mass black hole or intermediate mass black hole, respectively. Besides, a significant correlation between the peak power of the episodic jet and the rate-of-increase of the X-ray luminosity dL x /dt during the rising phase of those outbursts is also found, following log P jet = (2.0 ± 0.4) + (0.7 ± 0.2) × log dL x /dt. In GX 339−4 and H 1743−322 in which data for two outbursts are available, measurements of the peak radio power of the episodic jet and the X-ray peak luminosity (and its rate-of-change) shows similar positive correlations between outbursts, which demonstrate the dominant role of accretion over black hole spin in generating episodic jet power. On the other hand, no significant difference is seen among the systems with different measured black hole spin in current sample. This implies that the power of the episodic jet is strongly affected by non-stationary accretion instead of black hole spin characterized primarily by the rate-of-change of the mass accretion rate.

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Bright radio emission from an ultraluminous stellar-mass microquasar in M 31

Cited by 118 publications

References 37 publications

Irradiated, colour-temperature-corrected accretion discs in ultraluminous X-ray sources

Irradiated, colour-temperature-corrected accretion discs in ultraluminous X-ray sources

Large decay of X-ray flux in 2XMM J123103.2+110648: evidence for a tidal disruption event

Discovery of the correlation between peak episodic jet power and X-ray peak luminosity of the soft state in black hole transients

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