Radio lobes and X-ray hotspots in the microquasar S26

Soria, Roberto; Pakull, M. W.; Broderick, J. W.; Corbel, S.; Motch, C.

doi:10.1111/j.1365-2966.2010.17360.x

Cited by 63 publications

(91 citation statements)

References 57 publications

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“…Kaaret et al 2010), the supersoft ULX, M101 (Kong & Di Stefano 2005;Shen et al 2015), and the UV excess of SS433 (Dolan et al 1997). As the X-ray luminosity is expected to be low, the source may not fall into the empirical class of bright or even faint ULXs (see as possible examples Soria et al 2010Soria et al , 2014). Whilst we may not expect these to feature in ULX population studies, they represent an important set of 'hidden' ULXs, should provide interesting diagnostics for the winds (Middleton & Maccarone, in preparation) and are a necessary component of any model which hopes to describe the entire population.…”

Section: Source/population Evolution: Spectral Hardness Versus Variabmentioning

confidence: 99%

A spectral-timing model for ULXs in the supercritical regime

Middleton¹,

Heil

Pintore

et al. 2015

Monthly Notices of the Royal Astronomical Society

189

298

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Additional information: Use policyThe full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-prot purposes provided that:• a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders.Please consult the full DRO policy for further details. ABSTRACTUltraluminous X-ray sources (ULXs) with luminosities lying between ∼3 × 10 39 and 2 × 10 40 erg s −1 represent a contentious sample of objects as their brightness, together with a lack of unambiguous mass estimates for the vast majority of the central objects, leads to a degenerate scenario where the accretor could be a stellar remnant (black hole or neutron star) or intermediate-mass black hole (IMBH). Recent, high-quality observations imply that the presence of IMBHs in the majority of these objects is unlikely unless the accretion flow somehow deviates strongly from expectation based on objects with known masses. On the other hand, physically motivated models for supercritical inflows can re-create the observed X-ray spectra and their evolution, although have been lacking a robust explanation for their variability properties. In this paper, we include the effect of a partially inhomogeneous wind that imprints variability on to the X-ray emission via two distinct methods. The model is heavily dependent on both inclination to the line of sight and mass accretion rate, resulting in a series of qualitative and semiquantitative predictions. We study the time-averaged spectra and variability of a sample of well-observed ULXs, finding that the source behaviours can be explained by our model in both individual cases as well as across the entire sample, specifically in the trend of hardness-variability power. We present the covariance spectra for these sources for the first time, which shed light on the correlated variability and issues associated with modelling broad ULX spectra.Key words: accretion, accretion discs -X-rays: binaries. I N T RO D U C T I O NUltraluminous X-ray sources (ULXs) have been widely observed in the local Universe, with inferred isotropic luminosities above 10 39 erg s −1 (Roberts 2007;Feng & Soria 2011). Those below ∼3 × 10 39 erg s −1 can be readily associated with accretion on to stellar mass black holes (BHs) (∼10 M ) accreting close to or at their Eddington limit (see Sutton, Roberts & Middleton 2013, and references therein). There is now strong evidence to support this assertion, with the discovery of extremely bright ballistic jets from a ULX in M31 Middleton, Miller-Jones & Fender 2014b), which unambiguously links the flow with Eddington rate accretion (Fender, Belloni & Gallo 2004), and the first dynamical mass measurement of the compact object in a ULX, from M101 E-mail: mjm@ast.cam.ac.uk ULX-1 (Liu et al. 2013). Ob...

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Section: Source/population Evolution: Spectral Hardness Versus Variabmentioning

confidence: 99%

A spectral-timing model for ULXs in the supercritical regime

Middleton¹,

Heil

Pintore

et al. 2015

Monthly Notices of the Royal Astronomical Society

189

298

View full text Add to dashboard Cite

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“…2 right), that corresponds to a physical scale of ∼350 pc at 95 Mpc. Some of the largest microquasar and ULX radio bubbles, like S26 and IC 342 X-1 (Soria et al 2010;Cseh et al 2012), have a size of ∼ 200 − 300 pc and a high radio luminosity of LR ≃ 2 × 10 35 erg/s that would correspond to ∼3 µJy at a distance of HLX-1. These sources would not be resolved and would not reach our detection threshold.…”

Section: Permanent Emission: Radio Bubble or Star Formation?mentioning

confidence: 99%

On the radio properties of the intermediate-mass black hole candidate ESO 243-49 HLX-1

Cseh

Webb

Godet

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We present follow-up radio observations of ESO 243-49 HLX-1 from 2012 using the Australia Telescope Compact Array (ATCA) and the Karl G. Jansky Very Large Array (VLA). We report the detection of radio emission at the location of HLX-1 during its hard X-ray state using the ATCA. Assuming that the 'Fundamental Plane' of accreting black holes is applicable, we provide an independent estimate of the black hole mass of M BH 2.86 M ⊙ at 90% confidence. However, we argue that the detected radio emission is likely to be Doppler-boosted and our mass estimate is an upper limit. We discuss other possible origins of the radio emission such as being due to a radio nebula, star formation, or later interaction of the flares with the large-scale environment. None of these were found adequate. The VLA observations were carried out during the X-ray outburst. However, no new radio flare was detected, possibly due to a sparse time sampling. The deepest, combined VLA data suggests a variable radio source and we briefly discuss the properties of the previously detected flares and compare them with microquasars and active galactic nuclei.

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“…Other possible associations, like a single X-ray binary (such as CygX-3; Merloni et al 2003;Reines et al 2011) or an ultraluminous X-ray nebula (such as S26 and/or IC342X-1; Soria et al 2010;Cseh et al 2012), do not fit to the measured flux density of the persistent radio emission and/or the observed size by several orders of magnitude.…”

mentioning

confidence: 99%

The Repeating Fast Radio Burst FRB 121102 as Seen on Milliarcsecond Angular Scales

Marcote

Paragi

Hessels

et al. 2017

ApJL

385

436

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The millisecond-duration radio flashes known as fast radio bursts (FRBs) represent an enigmatic astrophysical phenomenon. Recently, the sub-arcsecond localization (∼100 mas precision) of FRB121102 using the Very Large Array has led to its unambiguous association with persistent radio and optical counterparts, and to the identification of its host galaxy. However, an even more precise localization is needed in order to probe the direct physical relationship between the millisecond bursts themselves and the associated persistent emission. Here, we report very-long-baseline radio interferometric observations using the European VLBI Network and the 305 m Arecibo telescope, which simultaneously detect both the bursts and the persistent radio emission at milliarcsecond angular scales and show that they are co-located to within a projected linear separation of 40 pc (12 mas angular separation, at 95% confidence). We detect consistent angular broadening of the bursts and persistent radio source (∼2-4 mas at 1.7 GHz), which are both similar to the expected Milky Way scattering contribution. The persistent radio source has a projected size constrained to be  0.7 pc (0.2 mas angular extent at 5.0 GHz) and a lower limit for the brightness temperature of T 5 10 K b 7´. Together, these observations provide strong evidence for a direct physical link between FRB121102 and the compact persistent radio source. We argue that a burst source associated with a low-luminosity active galactic nucleus or a young neutron star energizing a supernova remnant are the two scenarios for FRB121102 that best match the observed data.

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Radio lobes and X-ray hotspots in the microquasar S26

Cited by 63 publications

References 57 publications

A spectral-timing model for ULXs in the supercritical regime

A spectral-timing model for ULXs in the supercritical regime

On the radio properties of the intermediate-mass black hole candidate ESO 243-49 HLX-1

The Repeating Fast Radio Burst FRB 121102 as Seen on Milliarcsecond Angular Scales

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