Astrophysical implications of gravitational microlensing of gravitational waves

Paolis, F. De; Ingrosso, G.; Nucita, A. A.

doi:10.1051/0004-6361:20000304

Cited by 16 publications

(19 citation statements)

References 27 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…1) We generate the FFP distance from the observer L D , based on the thin disk FFP spatial distributions, which is assumed to follow that of the stars (Gilmore et al 1989, De Paolis et al 2001, Hafizi et al 2004. The galactic coordinates of the line of sight toward the Galactic bulge are considered ( 1.1 l  o , ( 1 100)…”

Section: Monte Carlo Calculations and Resultsmentioning

confidence: 99%

The astrometric signal of microlensing events caused by free floating planets

Hamolli

Hafizi

Paolis

et al. 2018

Astrophys Space Sci

View full text Add to dashboard Cite

Astrometric observations of microlensing events can be used to obtain important information about lenses. During these events, the shift of the position of the multiple image centroid with respect to the source star location can be measured. This effect, which is expected to occur on scales from micro-arcseconds to milliarcseconds, depends on the lens-source-observer system physical parameters. Here, we consider the astrometric and photometric observations by space and ground-based telescopes of microlensing events towards the Galactic bulge caused by free floating planets (FFPs). We show that the efficiency of astrometric signal on photometrically detected microlensing events tends to increase for higher FFP masses in our Galaxy. In addition, we estimate that during five years of the Gaia observations, about a dozen of microlensing events caused by FFPs are expected to be detectable.

show abstract

Section: Monte Carlo Calculations and Resultsmentioning

confidence: 99%

The astrometric signal of microlensing events caused by free floating planets

Hamolli

Hafizi

Paolis

et al. 2018

Astrophys Space Sci

View full text Add to dashboard Cite

show abstract

“…Consequently, the lensed source is always seen as an amplitude amplification (i.e. as a microlensing event) and the observed amplitude, at the frequency ω n , is (De Paolis et al 2001)…”

Section: Discussionmentioning

confidence: 99%

Astrophysical implications of binary black holes in BL Lacertae objects

Paolis

Ingrosso

Nucita

2002

A&A

Self Cite

View full text Add to dashboard Cite

Abstract. Some BL Lacertae objects show a periodic behaviour in their light curves that is often attributed to the orbital motion of a central binary black hole system. On this basis, and assuming a circular orbit, Rieger & Mannheim (2000) have recently proposed a method to determine the orbital parameters of the binary system from the observed quantities, i.e. the signal periodicity, the flux ratio between maximum and minimum signal and the power law spectral index of the photon flux. However, since these binary black holes are expected to originate from galactic mergers, they could well be on eccentric orbits, which might not circularize for a substantial time. We therefore generalize the treatment proposed by Rieger & Mannheim (2000) by taking into account the effect of the orbital eccentricity of the binary system. We apply the model to three well-observed Markarian objects: MKN 501, MKN 421 and MKN 766 that most likely host a binary system in their centers. Some astrophysical implications of this model are also investigated with particular emphasis to the gravitational radiation emission from the binary black holes. Under particular conditions (e.g. for some values of the orbital separation, eccentricity and Lorentz factor) one can obtain signals above the sensitivity threshold of the LISA detector.

show abstract

“…This topic has been addressed in the literature by many authors with various points of view: cosmological waveguides for GW [12], GW detection using gravitational lenses as detectors [13] and finally, microlensing [14] and macrolensing [15,16] of gravitational radiation in the high frequency approximation as well as in the diffraction case [17,18]. In this article we use the same approach as Ref.…”

Section: Introductionmentioning

confidence: 99%

Increase of the Number of Detectable Gravitational Waves Signals Due to Gravitational Lensing

Varvella

Angonin

Tourrenc

2004

General Relativity and Gravitation

View full text Add to dashboard Cite

This article deals with the gravitational lensing (GL) of gravitational waves (GW). We compute the increase in the number of detected GW events due to GL. First, we check that geometrical optics is valid for the GW frequency range on which Earth-based detectors are sensitive, and that this is also partially true for what concerns the future space-based interferometer LISA. To infer this result, both the diffraction parameter and a cut-off frequency are computed. Then, the variation in the number of GW signals is estimated in the general case, and applied to some lens models: point mass lens and singular isothermal sphere (SIS profile). An estimation of the magnification factor has also been done for the softened isothermal sphere and for the King profile. The results appear to be strongly model-dependent, but in all cases the increase in the number of detected GW signals is negligible. The use of time delays among images is also investigated.

show abstract

Astrophysical implications of gravitational microlensing of gravitational waves

Cited by 16 publications

References 27 publications

The astrometric signal of microlensing events caused by free floating planets

The astrometric signal of microlensing events caused by free floating planets

Astrophysical implications of binary black holes in BL Lacertae objects

Increase of the Number of Detectable Gravitational Waves Signals Due to Gravitational Lensing

Contact Info

Product

Resources

About