Polarization in binary microlensing events

Ingrosso, G.; Paolis, F. De; Nucita, A. A.; Strafella, F.; Novati, S. Calchi; Jetzer, Ph.; Liuzzi, Giuliano

doi:10.1088/0031-8949/89/8/084001

Cited by 13 publications

(12 citation statements)

References 33 publications

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“…It shows that the source crossed the tip of the caustic. We note that finite-source effects could also have been detected through specific features of polarization curves, if a polarization observation of the event were conducted (Ingrosso et al 2012(Ingrosso et al , 2014.…”

Section: Discussionmentioning

confidence: 93%

OGLE-2014-BLG-1112LB: A Microlensing Brown Dwarf Detected through the Channel of a Gravitational Binary-lens Event

Han

Udalski

Bozza

et al. 2017

ApJ

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Due to the nature of the gravitational field, microlensing, in principle, provides an important tool for detecting faint and even dark brown dwarfs. However, the number of identified brown dwarfs is limited due to the difficulty of the lens mass measurement that is needed to check the substellar nature of the lensing object. In this work, we report a microlensing brown dwarf discovered from an analysis of the gravitational binary-lens event OGLE-2014-BLG-1112. We identify the brown dwarf nature of the lens companion by measuring the lens mass from the detections of both microlens-parallax and finite-source effects. We find that the companion has a mass of ´- ( ) M 3.03 0.78 10 2 and it is orbiting a solar-type primary star with a mass of   M 1.07 0.28. The estimated projected separation between the lens components is 9.63±1.33 au and the distance to the lens is 4.84±0.67 kpc. We discuss the usefulness of space-based microlensing observations for detecting brown dwarfs through the channel of binary-lens events.

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Section: Discussionmentioning

confidence: 93%

OGLE-2014-BLG-1112LB: A Microlensing Brown Dwarf Detected through the Channel of a Gravitational Binary-lens Event

Han

Udalski

Bozza

et al. 2017

ApJ

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“…If it is so, it will be the first exoplanet in another galaxy [44][45][46][47]. As it was noted [48][49][50] polarization observations for pixel lensing event play an extremely important role to clarify parameters of microlenses and sources which are giant stars for pixel lensing events (see also [51] for a review).…”

Section: Gravitational Lensingmentioning

confidence: 99%

Graviton mass bounds from an analysis of bright star trajectories at the Galactic Center

2017

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Abstract. In February 2016 the LIGO & VIRGO collaboration reported the discovery of gravitational waves in merging black holes, therefore, the team confirmed GR predictions about an existence of black holes and gravitational waves in the strong gravitational field limit. Moreover, in their papers the joint LIGO & VIRGO team presented an upper limit on graviton mass such as m g < 1.2 × 10 −22 eV . So, the authors concluded that their observational data do not show any violation of classical general relativity. We show that an analysis of bright star trajectories could constrain graviton mass with a comparable accuracy with accuracies reached with gravitational wave interferometers and the estimate is consistent with the one obtained by the LIGO & VIRGO collaboration. This analysis gives an opportunity to treat observations of bright stars near the Galactic Center as a useful tool to obtain constraints on the fundamental gravity law such as modifications of the Newton gravity law in a weak field approximation. In that way, based on a potential reconstruction at the Galactic Center we obtain bounds on a graviton mass.

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“…It has been shown that polarization measurements could resolve degeneracies in theoretical models of microlensing events [85]. Calculations of polarization curves for microlensing events with features in the light curves induced by the presence of an exoplanet and observed towards the Galactic bulge have been done [87,88,89,90,91]. We use simple polarization and limb darkening models developed by [92], however, improved models are also developed taking into account radiative transfer in spectral lines, see for instance simulation results developed for Sun [93].…”

Section: Polarization Curves For Microlens Systems With Exoplanetsmentioning

confidence: 99%

Theoretical estimations of future polarization observations for exoplanery searches with gravitational microlensing

Ingrosso¹,

Paolis²,

Nucita³

et al. 2015

Proceedings of XXII International Baldin Seminar on High Energy Physics Problems — PoS(Baldin ISHEPP XXII)

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There are different methods for finding exoplanets such as radial spectral shifts, astrometrical measurements, transits, timing etc. Gravitational microlensing (including pixel-lensing) is among the most promising techniques with the potentiality of detecting Earth-like planets at distances about a few astronomical units from their host star or near the so-called snow line with a temperature in the range 0 − 100 0 C on a solid surface of an exoplanet. We emphasize the importance of polarization measurements which can help to resolve degeneracies in theoretical models. In particular, the polarization angle could give additional information about the relative position of the lens with respect to the source.

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Polarization in binary microlensing events

Cited by 13 publications

References 33 publications

OGLE-2014-BLG-1112LB: A Microlensing Brown Dwarf Detected through the Channel of a Gravitational Binary-lens Event

OGLE-2014-BLG-1112LB: A Microlensing Brown Dwarf Detected through the Channel of a Gravitational Binary-lens Event

Graviton mass bounds from an analysis of bright star trajectories at the Galactic Center

Theoretical estimations of future polarization observations for exoplanery searches with gravitational microlensing

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