Revisiting the dynamical case for a massive black hole in IC10 X-1

Laycock, S.; Maccarone, Thomas J.; Christodoulou, Dimitris M.

doi:10.1093/mnrasl/slv082

Cited by 54 publications

(49 citation statements)

References 39 publications

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“…It is thus expected that lowmetallicity stars can produce significantly higher black hole masses than solar-metallicity stars. The heaviest stellar-mass black hole known in our Galaxy is only M ≈ 15 M ⊙ (see [103]; note that previous estimates of the mass of the black hole in IC10 X-1 are unreliable [104]), and the best current thinking is that to produce ∼ 30 M ⊙ black holes the metallicity must be less than ∼ 10 − 50% of solar. In particular, [94] showed that lower metallicities increase the likely masses of black holes and increase greatly the rate of gravitational wave detections.…”

Section: Implications For Black Hole Binary Formationmentioning

confidence: 98%

Implications of the gravitational wave event GW150914

Miller

2016

Gen Relativ Gravit

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The era of gravitational-wave astronomy began on 14 September 2015, when the LIGO Scientific Collaboration detected the merger of two ∼ 30 M ⊙ black holes at a distance of ∼ 400 Mpc. This event has facilitated qualitatively new tests of gravitational theories, and has also produced exciting information about the astrophysical origin of black hole binaries. In this review we discuss the implications of this event for gravitational physics and astrophysics, as well as the expectations for future detections. In brief: (1) because the spins of the black holes could not be measured accurately and because mergers are not well calculated for modified theories of gravity, the current analysis of GW150914 does not place strong constraints on gravity variants that change only the generation of gravitational waves, but (2) it does strongly constrain alterations of the propagation of gravitational waves and alternatives to black holes. Finally, (3) many astrophysical models for the origin of heavy black hole binaries such as the GW150914 system are in play, but a reasonably robust conclusion that was reached even prior to the detection is that the environment of such systems needs to have a relatively low abundance of elements heavier than helium.

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Section: Implications For Black Hole Binary Formationmentioning

confidence: 98%

Implications of the gravitational wave event GW150914

Miller

2016

Gen Relativ Gravit

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“…The first unambiguous eclipsing behavior in a candidate BH X-ray binary outside the Milky Way was found in IC 10 X-1, located in a Local Group dwarf galaxy, with a Wolf-Rayet donor star, a binary period of 1.45 days, and an X-ray luminosity » L 10 X 38 erg s −1 (Prestwich et al 2007;Laycock et al 2015a;Steiner et al 2016). For IC 10 X-1, it is still disputed whether the accreting compact object is a BH or a neutron star (Laycock et al 2015b). Outside the Local Group, NGC 300 X-1 ( »Ĺ 5 10 X 38 erg s −1 ; binary period »33 hr) shows X-ray dips, consistent with occultation from geometrically thick structures in the outer disk, or absorption in the wind of the donor star, but not with true eclipses (Binder et al 2015).…”

Section: Table 11mentioning

confidence: 99%

Two Eclipsing Ultraluminous X-Ray Sources in M51

Urquhart

Soria

2016

ApJ

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We present the discovery, from archival Chandra and XMM-Newton data, of X-ray eclipses in two ultraluminous X-ray sources (ULXs), located in the same region of the galaxy M51: CXOM51 J132940.0+471237 (ULX-1, for simplicity) and CXOM51 J132939.5+471244 (ULX-2). Three eclipses were detected for ULX-1 and two for ULX-2. The presence of eclipses puts strong constraints on the viewing angle, suggesting that both ULXs are seen almost edge-on and are certainly not beamed toward us. Despite the similar viewing angles and luminosities ( »Ĺ 2 10 X 39 erg s −1 in the 0.3-8 keV band for both sources), their X-ray properties are different. ULX-1 has a soft spectrum, well fitted by Comptonization emission from a medium with electron temperature » kT 1 keV e . ULX-2 is harder, well fitted by a slim disk with » kT 1.5 in -1.8 keV and normalization consistent with a ∼10 M e black hole. ULX-1 has a significant contribution from multi-temperature thermal-plasma emission ( »Ĺ 2 10 X,mekal 38 erg s −1 ). About 10% of this emission remains visible during the eclipses, proving that the emitting gas comes from a region slightly more extended than the size of the donor star. From the sequence and duration of the Chandra observations in and out of eclipse, we constrain the binary period of ULX-1 to be either »6.3 days, or ≈12.5-13 days. If the donor star fills its Roche lobe (a plausible assumption for ULXs), both cases require an evolved donor, most likely a blue supergiant, given the young age of the stellar population in that Galactic environment.

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“…Owing to the unique challenges of observing the winddominated Wolf-Rayet companions, the masses of the compact objects in these systems are rather uncertain and, indeed, the presence of a neutron star cannot be ruled out (Binder et al 2015;Laycock et al 2015). Finally, we should also mention ultraluminous X-ray sources (ULXs), systems with X-ray luminosities that are greater than the Eddington limit for a 10 M BH.…”

Section: Introductionmentioning

confidence: 99%

BlackCAT: A catalogue of stellar-mass black holes in X-ray transients

Corral-Santana

Casares

Muñoz‐Darias

et al. 2016

A&A

437

364

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Aims. During the last ∼50 years, the population of black hole candidates in X-ray binaries has increased considerably, with 59 Galactic objects being detected in transient low-mass X-ray binaries, as well as a few in persistent systems (including ∼5 extragalactic binaries). Methods. We collect near-infrared, optical, and X-ray information spread over hundreds of references to study the population of black holes in X-ray transients as a whole.Results. We present the most updated catalogue of black hole transients. This contains X-ray, optical, and near-infrared observations, together with their astrometric and dynamical properties. The catalogue provides new and useful information in both statistical and observational parameters and provides a thorough and complete overview of the black hole population in the Milky Way. Analysing the distances and spatial distribution of the observed systems, we estimate a total population of ∼1300 Galactic black hole transients. This means that we have only discovered less than ∼5% of the total Galactic distribution.

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Revisiting the dynamical case for a massive black hole in IC10 X-1

Cited by 54 publications

References 39 publications

Implications of the gravitational wave event GW150914

Implications of the gravitational wave event GW150914

Two Eclipsing Ultraluminous X-Ray Sources in M51

BlackCAT: A catalogue of stellar-mass black holes in X-ray transients

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