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

Cseh, D.; Webb, N.; Godet, O.; Barret, D.; Corbel, S.; Coriat, M.; Falcke, H.; Farrell, Sean; Körding, Elmar; Lenc, E.; Wrobel, J. M.

doi:10.1093/mnras/stu2363

Cited by 42 publications

(43 citation statements)

References 90 publications

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“…3). From the radio emission and applying the fundamental plane of accreting BHs, a BH mass of 9 × (10 3 − 10 4 ) was estimated by Webb et al (2012) and an upper limit of 2.8 × 10 6 M by Cseh et al (2015a). Cseh et al (2015a) suggested that the radio emission is Dopplerboosted and that HLX-1 could be an outlier on the fundamental plane.…”

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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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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“…While the formation channel of IMBHs is unknown, there are a small number of proposed scenarios: (i) the direct collapse of massive first-generation, lowmetallicity Population III stars [57][58][59][60], (ii) runaway mergers of massive main sequence stars in dense stellar clusters [61][62][63][64][65], (iii) the accretion of residual gas onto stellar-mass black holes [66], and (iv) chemically homogeneous evolution [67]. 6 It has been suggested that the most likely locations to find IMBHs are at the centers of GCs [68][69][70][71][72][73][74][75][76][77][78][79][80]. It follows that these are also the most likely places to find IMBHBs.…”

Section: Astrophysical Implicationsmentioning

confidence: 99%

Search for intermediate mass black hole binaries in the first observing run of Advanced LIGO

Abbott

Jawahar

Lockerbie³

et al. 2017

Phys. Rev. D

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During their first observational run, the two Advanced LIGO detectors attained an unprecedented sensitivity, resulting in the first direct detections of gravitational-wave signals produced by stellar-mass binary black hole systems. This paper reports on an all-sky search for gravitational waves (GWs) from merging intermediate mass black hole binaries (IMBHBs). The combined results from two independent search techniques were used in this study: the first employs a matched-filter algorithm that uses a bank of filters covering the GW signal parameter space, while the second is a generic search for GW transients (bursts). No GWs from IMBHBs were detected; therefore, we constrain the rate of several classes of IMBHB mergers. The most stringent limit is obtained for black holes of individual mass 100 M ⊙ , with spins aligned with the binary orbital angular momentum. For such systems, the merger rate is constrained to be less than 0.93 Gpc −3 yr −1 in comoving units at the 90% confidence level, an improvement of nearly 2 orders of magnitude over previous upper limits.

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“…In the microquasar GRS 1915+105, often compared to ULXs for its peak luminosity, steady jets are present during the hard so-called "plateau" state and ejection events during state changes (Mirabel and Rodríguez 1994;. Jets are associated with HLXs during state transitions, and this is considered evidence of the sub-Eddington regime, and so of their nature as IMBH (Cseh et al 2015a;Mezcua et al 2015). Only one sULXs, Holmberg II X-1, has been Fig.…”

Section: Jets and Outflowsmentioning

confidence: 99%

Ultraluminous X‐ray sources: Three exciting years

Bachetti

2016

Astron Nachr

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The extreme extragalactic sources known as Ultraluminous X-ray Sources (ULX) represent a unique testing environment for compact objects population studies and the accretion process. Their nature has long been disputed. Their luminosity, well above the Eddington luminosity for a stellar-mass black hole, can imply the presence of an intermediate-mass black hole or a stellar black hole accreting above the Eddington limit. Both these interpretations are important to understand better the accretion process and the evolution of massive black holes. The last few years have seen a dramatic improvement of our knowledge of these sources. In particular, the super-Eddington interpretation for the bulk of the ULX population has gained a strong consensus. Nonetheless, exceptions to this general trend do exist, and in particular one ULX was shown to be a neutron star, and another was shown to be a very likely IMBH candidate. In this paper, I will review the progress done in the last few years.

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

Cited by 42 publications

References 90 publications

Observational evidence for intermediate-mass black holes

Observational evidence for intermediate-mass black holes

Search for intermediate mass black hole binaries in the first observing run of Advanced LIGO

Ultraluminous X‐ray sources: Three exciting years

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