Black Hole Powered Nebulae and a Case Study of the Ultraluminous X-Ray Source Ic 342 X-1

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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“…Cseh et al 2012), at low flux density levels. The individual runs are in principle suitable to look for flares from HLX-1.…”

Section: Vla Observationsmentioning

confidence: 97%

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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“…A BH mass of 5 × 10 4 M was estimated using the fundamental plane for accreting BHs, consistent with NGC 2276-3c containing an IMBH in the hard state . The detection of compact radio jets has suggested the presence of IMBHs in some other ULXs for which the fundamental plane provides a BH mass estimate in the IMBH regime (e.g., N4861-X2, N4088-X1, Mezcua & Lobanov 2011; IC342 X-1, Cseh et al 2012;N5457-X9, Mezcua et al 2013a). However, the luminosity of these ULXs being < 5 × 10 40 erg s −1 makes them also consistent with the super-Eddington accretion scenario.…”

Section: Ultraluminous X-ray Sourcesmentioning

confidence: 99%

Observational evidence for intermediate-mass black holes

Mezcua

2017

Int. J. Mod. Phys. D

268

219

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Intermediate-mass black holes (IMBHs), with masses in the range 100 − 10 6 M , are the link between stellar-mass BHs and supermassive BHs (SMBHs). They are thought to be the seeds from which SMBHs grow, which would explain the existence of quasars with BH masses of up to 10 10 M when the Universe was only 0.8 Gyr old. The detection and study of IMBHs has thus strong implications for understanding how SMBHs form and grow, which is ultimately linked to galaxy formation and growth, as well as for studies of the universality of BH accretion or the epoch of reionisation. Proving the existence of seed BHs in the early Universe is not yet feasible with the current instrumentation; however, those seeds that did not grow into SMBHs can be found as IMBHs in the nearby Universe. In this review I summarize the different scenarios proposed for the formation of IMBHs and gather all the observational evidence for the few hundreds of nearby IMBH candidates found in dwarf galaxies, globular clusters, and ultraluminous X-ray sources, as well as the possible discovery of a few seed BHs at high redshift. I discuss some of their properties, such as X-ray weakness and location in the BH mass scaling relations, and the possibility to discover IMBHs through high velocity clouds, tidal disruption events, gravitational waves, or accretion disks in active galactic nuclei. I finalize with the prospects for the detection of IMBHs with up-coming observatories.

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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.…”

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confidence: 97%

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

Marcote

Paragi

Hessels

et al. 2017

ApJL

389

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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Black Hole Powered Nebulae and a Case Study of the Ultraluminous X-Ray Source Ic 342 X-1

Cited by 90 publications

References 82 publications

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

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

Observational evidence for intermediate-mass black holes

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

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