The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs★

Wyrzykowski, Ł.; Skowron, J.; Kozłowski, S.; Udalski, A.; Szymański, M. K.; Kubiak, M.; Pietrzyński, G.; Szewczyk, O.; Ulaczyk, K.; Poleski, R.; Tisserand, Patrick

doi:10.1111/j.1365-2966.2011.19243.x

Cited by 196 publications

(198 citation statements)

References 37 publications

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“…In the LIGO region, microlensing (Alcock et al 1996Allsman et al 2001;Lasserre 2000;Tisserand et al 2007;Wyrzykowski et al 2011) and star cluster dynamics in the Eridanus II (Brandt 2016) and Segue I dwarf galaxies (Koushiappas & Loeb 2017) place the tightest constraints on PBH dark matter (Fig. 1).…”

Section: An Overview Of Constraints On Primordial Black Hole Dark Mattermentioning

confidence: 99%

Disentangling the Potential Dark Matter Origin of LIGO’s Black Holes

Magee

Hanna

2017

ApJL

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The nature of dark matter (DM) remains one of the biggest open questions in physics. One intriguing dark matter candidate, primordial black holes (PBHs), has faced renewed interest following LIGO's detection of gravitational waves from merging stellar mass black holes. While subsequent work has ruled out the possibility that dark matter could consist solely of black holes similar to those that LIGO has detected with masses above 10M , LIGO's connection to dark matter remains unknown. In this work we consider a distribution of primordial black holes that accounts for all of the dark matter, is consistent with all of LIGO's observations arising from primordial black hole binaries, and resolves tension in previous surveys of microlensing events in the Milky Way halo. The primordial black hole mass distribution that we consider offers an important prediction-LIGO may detect black holes smaller than have ever been observed with ∼ 1% of the black holes it detects having a mass less than the mass of our Sun and ∼ 10% with masses in the mass-gap. Approximately one year of operating advanced LIGO at design sensitivity should be adequate to begin to see a hint of a primordial black hole mass distribution. Detecting primordial black hole binaries below a solar mass will be readily distinguishable from other known compact binary systems, thereby providing an unambiguous observational window for advanced LIGO to pin down the nature of dark matter.

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Section: An Overview Of Constraints On Primordial Black Hole Dark Mattermentioning

confidence: 99%

Disentangling the Potential Dark Matter Origin of LIGO’s Black Holes

Magee

Hanna

2017

ApJL

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“…There is a window for PBHs to be DM if the BH mass is in the range 20 M M 100 M [8,9]. Lower masses are excluded by microlensing surveys [10][11][12]. Higher masses would disrupt wide binaries [9,13,14].…”

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confidence: 99%

Did LIGO Detect Dark Matter?

et al. 2016

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We consider the possibility that the black-hole (BH) binary detected by LIGO may be a signature of dark matter. Interestingly enough, there remains a window for masses 20 M M bh 100 M where primordial black holes (PBHs) may constitute the dark matter. If two BHs in a galactic halo pass sufficiently close, they radiate enough energy in gravitational waves to become gravitationally bound. The bound BHs will rapidly spiral inward due to emission of gravitational radiation and ultimately merge. Uncertainties in the rate for such events arise from our imprecise knowledge of the phase-space structure of galactic halos on the smallest scales. Still, reasonable estimates span a range that overlaps the 2 − 53 Gpc −3 yr −1 rate estimated from GW150914, thus raising the possibility that LIGO has detected PBH dark matter. PBH mergers are likely to be distributed spatially more like dark matter than luminous matter and have no optical nor neutrino counterparts. They may be distinguished from mergers of BHs from more traditional astrophysical sources through the observed mass spectrum, their high ellipticities, or their stochastic gravitational wave background. Next generation experiments will be invaluable in performing these tests.The nature of the dark matter (DM) is one of the most longstanding and puzzling questions in physics. Cosmological measurements have now determined with exquisite precision the abundance of DM [1, 2], and from both observations and numerical simulations we know quite a bit about its distribution in Galactic halos. Still, the nature of the DM remains a mystery. Given the efficacy with which weakly-interacting massive particlesfor many years the favored particle-theory explanationhave eluded detection, it may be warranted to consider other possibilities for DM. Primordial black holes (PBHs) are one such possibility [3-6].Here we consider whether the two ∼ 30 M black holes detected by LIGO [7] could plausibly be PBHs. There is a window for PBHs to be DM if the BH mass is in the range 20 M M 100 M [8,9]. Lower masses are excluded by microlensing surveys [10][11][12]. Higher masses would disrupt wide binaries [9,13,14]. It has been argued that PBHs in this mass range are excluded by CMB constraints [15,16]. However, these constraints require modeling of several complex physical processes, including the accretion of gas onto a moving BH, the conversion of the accreted mass to a luminosity, the self-consistent feedback of the BH radiation on the accretion process, and the deposition of the radiated energy as heat in the photon-baryon plasma. A significant (and difficult to quantify) uncertainty should therefore be associated with this upper limit [17], and it seems worthwhile to examine whether PBHs in this mass range could have other observational consequences.In this Letter, we show that if DM consists of ∼ 30 M BHs, then the rate for mergers of such PBHs falls within the merger rate inferred from GW150914. In any galactic halo, there is a chance two BHs will undergo a hard scatter, lose energy to a s...

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“…The observational result from this lensing is the magnification of light of the source object (Paczyński 1986). This method has been used for detection of possible MACHOs 1 in the Galactic halo and the observations of EROS, MACHO and OGLE groups for almost one decade in the direction of Large Magellanic Clouds revealed that MACHOs do not contribute in the dark matter budget of Galactic halo (Tisserand et al 2007;Wyrzykowski et al 2011;Moniez 2010). Also in recent years this method is used as a strong tool for detection of Earth-mass extrasolar planets beyond the snow line (Mao & Paczynski 1991;Gould et al 2010;Gaudi 2012).…”

Section: Introductionmentioning

confidence: 99%

Eclipsing negative-parity image of gravitational microlensing by a giant-lens star

Rahvar

2016

Mon. Not. R. Astron. Soc.

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Gravitational Microlensing has been used as a powerful tool for astrophysical studies and exoplanet detections. In the gravitational microlensing, we have two images with negative and positive parities. The negative-parity image is a fainter image and is produced at a closer angular separation with respect to the lens star. In the case of a red-giant lens star and large impact parameter of lensing, this image can be eclipsed by the lens star. The result would be dimming the flux receiving from the combination of the source and the lens stars and the light curve resembles to an eclipsing binary system. In this work, we introduce this phenomenon and propose an observational procedure for detecting this eclipse. The follow-up microlensing telescopes with lucky imaging camera or space-based telescopes can produce high resolution images from the events with reddish sources and confirm the possibility of blending due to the lens star. After conforming a red-giant lens star and source star, we can use the advance photometric methods and detect the relative flux change during the eclipse in the order of 10 −4 − 10 −3 . Observation of the eclipse provides the angular size of source star in the unit of Einstein angle and combination of this observation with the parallax observation enable us to calculate the mass of lens star. Finally, we analyzed seven microlensing event and show the feasibility of observation of this effect in future observations.

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The OGLE view of microlensing towards the Magellanic Clouds - IV. OGLE-III SMC data and final conclusions on MACHOs★

Cited by 196 publications

References 37 publications

Disentangling the Potential Dark Matter Origin of LIGO’s Black Holes

Disentangling the Potential Dark Matter Origin of LIGO’s Black Holes

Did LIGO Detect Dark Matter?

Eclipsing negative-parity image of gravitational microlensing by a giant-lens star

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