Black hole, neutron star and white dwarf candidates from microlensing with OGLE-III

Wyrzykowski, Ł.; Kostrzewa-Rutkowska, Z.; Skowron, J.; Rybicki, K.; Mróz, P.; Kozłowski, S.; Udalski, A.; Szymański, M. K.; Pietrzyński, G.; Ulaczyk, K.; Poleski, R.; Pawlak, M.; Iłkiewicz, Krystian; Rattenbury, N. J.

doi:10.1093/mnras/stw426

Cited by 156 publications

(177 citation statements)

References 61 publications

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“…They found no evidence for a gap in the mass of remnants between neutron stars and black holes as suggested by Belczynski et al (2012). We have estimated a mean mass for single/runaway black-holes from the sample of Wyrzykowski et al (2016). We have assumed the same minimum mass for an object to be a black hole as in our models of 3M⊙.…”

Section: Predicting the Remnant Masses And Sn Kick Velocitiesmentioning

confidence: 84%

“…Vertical lines indicate two widely used values for Solar metallicity. We also plot the mean mass of these Galactic black-hole binaries in the green square and the mean mass of the single black-hole candidates identified from gravitational microlensing by Wyrzykowski et al (2016) in the orange square. The two thin horizontal lines indicate the masses of the black holes from GW150914.…”

Section: Predicting the Remnant Masses And Sn Kick Velocitiesmentioning

confidence: 99%

“…Recently Wyrzykowski et al (2016) have detailed a number of candidate single compact remnants in the Galaxy discovered via gravitational microlensing. They found no evidence for a gap in the mass of remnants between neutron stars and black holes as suggested by Belczynski et al (2012).…”

Section: Predicting the Remnant Masses And Sn Kick Velocitiesmentioning

confidence: 99%

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bpass predictions for binary black hole mergers

Eldridge

Stanway

2016

Mon. Not. R. Astron. Soc.

270

225

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Using the Binary Population and Spectral Synthesis code BPASS, we have calculated the rates, timescales and mass distributions for binary black hole mergers as a function of metallicity. We consider these in the context of the recently reported 1st LIGO event detection. We find that the event has a very low probability of arising from a stellar population with initial metallicity mass fraction above Z = 0.010 (Z > ∼ 0.5 Z ⊙ ). Binary black hole merger events with the reported masses are most likely in populations below 0.008 (Z < ∼ 0.4 Z ⊙ ). Events of this kind can occur at all stellar population ages from 3 Myr up to the age of the universe, but constitute only 0.1 to 0.4 per cent of binary BH mergers between metallicities of Z = 0.001 to 0.008. However at metallicity Z = 10 −4 , 26 per cent of binary BH mergers would be expected to have the reported masses. At this metallicity the progenitor merger times can be close to ≈ 10Gyr and rotationallymixed stars evolving through quasi-homogeneous evolution, due to mass transfer in a binary, dominate the rate. The masses inferred for the black holes in the binary progenitor of GW 150914 are amongst the most massive expected at anything but the lowest metallicities in our models. We discuss the implications of our analysis for the electromagnetic follow-up of future LIGO event detections.

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Section: Predicting the Remnant Masses And Sn Kick Velocitiesmentioning

confidence: 84%

Section: Predicting the Remnant Masses And Sn Kick Velocitiesmentioning

confidence: 99%

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bpass predictions for binary black hole mergers

Eldridge

Stanway

2016

Mon. Not. R. Astron. Soc.

270

225

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“…Such long timescale events are of scientific importance for various reasons. First, lenses of these events are candidates of heavy stellar remnants such as neutron stars (NSs) and black holes (BHs) (Shvartzvald et al 2015;Wyrzykowski et al 2016). The event timescale, which is defined as the time for the source to cross the angular Einstein radius, θ E , of the lens, is related to the physical parameters of the lens system by…”

Section: Introductionmentioning

confidence: 99%

KMT-2016-BLG-2052L: Microlensing Binary Composed of M Dwarfs Revealed from a Very Long Timescale Event

Han

Jung

Shvartzvald

et al. 2018

ApJ

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We present the analysis of a binary microlensing event, KMT-2016-BLG-2052, for which the lensing-induced brightening of the source star lasted for two seasons. We determine the lens mass from the combined measurements of the microlens parallax, π E , and angular Einstein radius, θ E . The measured mass indicates that the lens is a binary composed of M dwarfs with masses of M 1 ∼0.34M e and M 2 ∼0.17M e . The measured relative lens-source proper motion of μ∼3.9masyr −1 is smaller than ∼5masyr −1 of typical Galactic lensing events, while the estimated angular Einstein radius of θ E ∼1.2mas is substantially greater than the typical value of ∼0.5mas. Therefore, it turns out that the long timescale of the event is caused by the combination of the slow μ and large θ E rather than the heavy mass of the lens. From the simulation of Galactic lensing events with very long timescales (t E 100 days), we find that the probabilities that long timescale events are produced by lenses with masses 1.0M e and 3.0M e are ∼19% and 2.6%, respectively, indicating that events produced by heavy lenses comprise a minor fraction of long timescale events. The results indicate that it is essential to determine lens masses by measuring both π E and θ E in order to firmly identify heavy stellar remnants, such as neutron stars and black holes.

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“…The microlensing technique can probe a variety of astronomical objects in a wide range of masses such as planets, neutron stars, brown dwarfs, and isolated black holes (Poindexter et al 2005;Dong et al 2007;Miyake et al 2012;Shvartzvald et al 2015;Wyrzykowski et al 2016). The microlensing technique can detect these faint or dark objects regardless of their luminosity levels, in sharp contrast to other methods, which as a matter of course are restricted to studying objects within their flux detection limits.…”

Section: Introductionmentioning

confidence: 99%

OGLE-2016-BLG-0168 Binary Microlensing Event: Prediction and Confirmation of the Microlens Parallax Effect from Space-based Observations

Shin¹,

Udalski²,

Yee³

et al. 2017

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The microlens parallax is a crucial observable for conclusively identifying the nature of lens systems in microlensing events containing or composed of faint (even dark) astronomical objects such as planets, neutron stars, brown dwarfs, and black holes. With the commencement of a new era of microlensing in collaboration with space-based observations, the microlens parallax can be routinely measured. In addition, space-based observations can provide opportunities to verify the microlens parallax measured from ground-only observations and to find a unique solution to the lensing light-curve analysis. Furthermore, since most space-based observations cannot cover the full light curves of lensing events, it is also necessary to verify the reliability of the information extracted from fragmentary space-based light curves. We conduct a test based on the microlensing event OGLE-2016-BLG-0168, created by a binary lens system consisting of almost equal mass M-dwarf stars, to demonstrate that it is possible to verify the microlens parallax and to resolve degeneracies using the space-based light curve even though the observations are fragmentary. Since space-based observatories will frequently produce fragmentary light curves due to their short observing windows, the methodology of this test will be useful for next-generation microlensing experiments that combine space-based and ground-based collaboration.

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Black hole, neutron star and white dwarf candidates from microlensing with OGLE-III

Cited by 156 publications

References 61 publications

bpass predictions for binary black hole mergers

bpass predictions for binary black hole mergers

KMT-2016-BLG-2052L: Microlensing Binary Composed of M Dwarfs Revealed from a Very Long Timescale Event

OGLE-2016-BLG-0168 Binary Microlensing Event: Prediction and Confirmation of the Microlens Parallax Effect from Space-based Observations

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