Constraining the masses of microlensing black holes and the mass gap with <i>Gaia</i> DR2

Wyrzykowski, Ł.; Mandel, Ilya

doi:10.1051/0004-6361/201935842

Cited by 139 publications

(117 citation statements)

References 93 publications

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“…Secondly, for events without caustic-crossings, the separation between the Earth and Roman's orbit at L2 will not be large enough to reveal a microlensing parallax measurement. Fortunately, for events with caustic-crossings the Earth-L2 separation yields a useful microlensing parallax measurement as Wyrzykowski et al (2020) demonstrate. Moreover, for events with anomalies due to terrestrial planets, the microlens parallax may be measurable even in the absence of caustic-crossing features (Gould, Gaudi & Han 2003).…”

mentioning

confidence: 88%

OGLE-2018-BLG-1428Lb: a Jupiter-mass planet beyond the snow line of a dwarf star

Kim

Chung

Udalski

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We present the analysis of the microlensing event OGLE-2018-BLG-1428, which has a short-duration (∼1 day) caustic-crossing anomaly. The event was caused by a planetary lens system with planet/host mass ratio q = 1.7 × 10−3. Thanks to the detection of the caustic-crossing anomaly, the finite source effect was well measured, but the microlens parallax was not constrained due to the relatively short timescale (tE = 24 days). From a Bayesian analysis, we find that the host star is a dwarf star $M_{\rm host}=0.43^{+0.33}_{-0.22} \ M_{\odot }$ at a distance $D_{\rm L}=6.22^{+1.03}_{-1.51}\ {\rm kpc}$ and the planet is a Jovian-mass planet $M_{\rm p}=0.77^{+0.77}_{-0.53} \ M_{\rm J}$ with a projected separation $a_{\perp }=3.30^{+0.59}_{-0.83}\ {\rm au}$. The planet orbits beyond the snow line of the host star. Considering the relative lens-source proper motion of $\mu _{\rm rel} = 5.58 \pm 0.38\ \rm mas\ yr^{-1}$, the lens can be resolved by adaptive optics with a 30m telescope in the future.

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confidence: 88%

OGLE-2018-BLG-1428Lb: a Jupiter-mass planet beyond the snow line of a dwarf star

Kim

Chung

Udalski

et al. 2021

Monthly Notices of the Royal Astronomical Society

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“…At such mass-loss rates single stars (or stars in wide non-interacting binaries) may form ∼40 M He cores with ∼20−30 M H-rich envelopes leading to massive BH formation even at high metallicity. Such massive BHs would be found either as single BHs through microlensing surveys (e.g., Wyrzykowski & Mandel 2020) or in wide binaries through radial velocity surveys (motion of the companion star). We note that such massive BHs would not necessarily add to either LIGO/Virgo or X-ray binary populations that form (at least in classical isolated binary evolution) from interacting binaries in which stars lose their H-rich envelopes (e.g., this study, Wiktorowicz et al 2014).…”

Section: Isolated Binary Evolutionmentioning

confidence: 99%

Evolutionary roads leading to low effective spins, high black hole masses, and O1/O2 rates for LIGO/Virgo binary black holes

Belczyński

Klencki

Fields

et al. 2020

A&A

391

375

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All ten LIGO/Virgo binary black hole (BH-BH) coalescences reported following the O1/O2 runs have near-zero effective spins. There are only three potential explanations for this. If the BH spin magnitudes are large, then: (i) either both BH spin vectors must be nearly in the orbital plane or (ii) the spin angular momenta of the BHs must be oppositely directed and similar in magnitude. Then there is also the possibility that (iii) the BH spin magnitudes are small. We consider the third hypothesis within the framework of the classical isolated binary evolution scenario of the BH-BH merger formation. We test three models of angular momentum transport in massive stars: a mildly efficient transport by meridional currents (as employed in the Geneva code), an efficient transport by the Tayler-Spruit magnetic dynamo (as implemented in the MESA code), and a very-efficient transport (as proposed by Fuller et al.) to calculate natal BH spins. We allow for binary evolution to increase the BH spins through accretion and account for the potential spin-up of stars through tidal interactions. Additionally, we update the calculations of the stellar-origin BH masses, including revisions to the history of star formation and to the chemical evolution across cosmic time. We find that we can simultaneously match the observed BH-BH merger rate density and BH masses and BH-BH effective spins. Models with efficient angular momentum transport are favored. The updated stellar-mass weighted gas-phase metallicity evolution now used in our models appears to be key for obtaining an improved reproduction of the LIGO/Virgo merger rate estimate. Mass losses during the pair-instability pulsation supernova phase are likely to be overestimated if the merger GW170729 hosts a BH more massive than 50 M⊙. We also estimate rates of black hole-neutron star (BH-NS) mergers from recent LIGO/Virgo observations. If, in fact. angular momentum transport in massive stars is efficient, then any (electromagnetic or gravitational wave) observation of a rapidly spinning BH would indicate either a very effective tidal spin up of the progenitor star (homogeneous evolution, high-mass X-ray binary formation through case A mass transfer, or a spin- up of a Wolf-Rayet star in a close binary by a close companion), significant mass accretion by the hole, or a BH formation through the merger of two or more BHs (in a dense stellar cluster).

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“…An important feature of this scenario is that it predicts the form of the PBH mass distribution precisely. We show that the expected form not only satisfies all the current astrophysical and cosmological constraints but also allows the PBHs to explain numerous observational conundra: (1) microlensing events towards the Galactic bulge generated by planet-mass objects with 1% of the CDM, well above most expectations for free-floating planets; (2) microlensing of quasars, including ones that are so misaligned with the lensing galaxy that the probability of lensing by a star is very low; (3) the unexpected high number of microlensing events towards the Galactic bulge by dark objects in the mass gap between 2 and 5 M [25], where stellar evolution models fail to form black holes [26]; (4) unexplained correlations in the source-subtracted X-ray and cosmic infrared background fluctuations [27]; (5) the non-observation of ultra-faint dwarf galaxies (UFDGs) below the critical radius of dynamical heating by PBHs [28]; (6) the mass, spins and coalescence rates for the black holes found by LIGO/Virgo [2]; (7)…”

Section: Extending the Scenario To The Thermal History Of The Universementioning

confidence: 95%

Primordial black holes and the origin of the matter–antimatter asymmetry

García-Bellido

2019

Phil. Trans. R. Soc. A.

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We review here a new scenario of hot spot electroweak baryogenesis where the local energy released in the gravitational collapse to form primordial black holes (PBHs) at the quark-hadron (QCD) epoch drives over-the-barrier sphaleron transitions in a far from equilibrium environment with just the standard model CP violation. Baryons are efficiently produced in relativistic collisions around the black holes and soon redistribute to the rest of the universe, generating the observed matter–antimatter asymmetry well before primordial nucleosynthesis. Therefore, in this scenario there is a common origin of both the dark matter to baryon ratio and the photon to baryon ratio. Moreover, the sudden drop in radiation pressure of relativistic matter at H 0 / W ± / Z 0 decoupling, the QCD transition and e + e − annihilation enhances the probability of PBH formation, inducing a multi-modal broad mass distribution with characteristic peaks at 10 −6 , 1, 30 and 10 6 M ⊙ , rapidly falling at smaller and larger masses, which may explain the LIGO–Virgo black hole mergers as well as the OGLE-GAIA microlensing events, while constituting all of the cold dark matter today. We predict the future detection of binary black hole (BBH) mergers in LIGO with masses between 1 and 5 M ⊙ , as well as above 80 M ⊙ , with very large mass ratios. Next generation gravitational wave and microlensing experiments will be able to test this scenario thoroughly. This article is part of a discussion meeting issue ‘Topological avatars of new physics’.

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Constraining the masses of microlensing black holes and the mass gap with Gaia DR2

Cited by 139 publications

References 93 publications

OGLE-2018-BLG-1428Lb: a Jupiter-mass planet beyond the snow line of a dwarf star

OGLE-2018-BLG-1428Lb: a Jupiter-mass planet beyond the snow line of a dwarf star

Evolutionary roads leading to low effective spins, high black hole masses, and O1/O2 rates for LIGO/Virgo binary black holes

Primordial black holes and the origin of the matter–antimatter asymmetry

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