Mutual Interference and Structural Properties of Object Images in the Vicinity of the Gravitational Lens CUSP Point

Mandzhos, A. V.

doi:10.1017/s0074180900110605

Cited by 4 publications

(5 citation statements)

References 1 publication

Supporting

Mentioning

Contrasting

Order By: Relevance

“…However as suggested by Ruffa (1999), the focused region by the gravitational lensing would have a relatively large area because of the diffraction, so that the lensing probability will increase. Since the gravitational waves from the compact binaries are coherent, the interference is also important (Mandzhos 1981, Ohanian 1983, Schneider & Schmid-Burgk 1985, Deguchi & Watson 1986b, Peterson & Falk 1991. Thus we expect that the wave effects (diffraction and interference) would provide much information about the lens objects.…”

Section: Introductionmentioning

confidence: 96%

Wave Effects in the Gravitational Lensing of Gravitational Waves from Chirping Binaries

Takahashi¹,

Nakamura²

2003

ApJ

315

469

View full text Add to dashboard Cite

In the gravitational lensing of gravitational waves, wave optics should be used instead of geometrical optics when the wavelength of the gravitational waves is longer than the Schwarzschild radius of the lens mass M L . For gravitational lensing of chirp signals from the coalescence of supermassive black holes at redshift z S $ 1 relative to the Laser Interferometer Space Antenna, the wave effects become important for a lens mass smaller than $10 8 M . For such cases, we compute how accurately we can extract the mass of the lens and the source position from the lensed signal. We consider two simple lens models: the point-mass lens and the SIS (singular isothermal sphere). We find that the lens mass and the source position can be determined to within $0.1% of ½ðS=NÞ=10 3 À1 for a lens mass larger than 10 8 M and e10% of ½ðS=NÞ=10 3 À1 for a lens mass smaller than 10 7 M because of the diffraction effect, where S/N is the signal-to-noise ratio of the unlensed chirp signals. For the SIS model, if the source position is outside the Einstein radius, only a single image exists in the geometrical optics approximation, so that the lens parameters cannot be determined, while in the wave optics cases we find that the lens mass can be determined even for M L < 10 8 M . For the pointmass lens, one can extract the lens parameters even if the source position is far outside the Einstein radius. As a result, the lensing cross section is an order of magnitude larger than that for the usual strong lensing of light.

show abstract

Section: Introductionmentioning

confidence: 96%

Wave Effects in the Gravitational Lensing of Gravitational Waves from Chirping Binaries

Takahashi¹,

Nakamura²

2003

ApJ

315

469

View full text Add to dashboard Cite

show abstract

“…Since the Schwarzschild radius of PBH is comparable to the photon wavelength, the wave nature of electromagnetic radiation has to be taken into account. In such a case, lensing caused by PBHs introduces an interferometry pattern in the energy spectrum of the lensed object [9]. The effect is called ''femtolensing'' [10] due to the $10 À15 arcseconds angular distance between the images of a source lensed by a 10 18 g lens.…”

Section: Introductionmentioning

confidence: 99%

New constraints on primordial black holes abundance from femtolensing of gamma-ray bursts

2012

View full text Add to dashboard Cite

The abundance of primordial black holes is currently significantly constrained in a wide range of masses. The weakest limits are established for the small mass objects where the small intensity of the associated physical phenomenon provides a challenge for current experiments. We used gamma-ray bursts with known redshifts detected by the Fermi Gamma-ray Burst Monitor (GBM) to search for the femtolensing effects caused by compact objects. The lack of femtolensing detection in the GBM data provides new evidence that primordial black holes in the mass range 10 17 -10 20 g do not constitute a major fraction of dark matter.

show abstract

“…The possibility of interference effects in gravitational lensing has been considered by several authors (Mandzhos 1981;Schneider & Schmidt-Burgk 1985;Deguchi & Watson 1986;Peterson & Falk 1991;Gould 1992;Stanek, Paczyński, & Goodman 1993). Of particular interest are diffractive variations in flux with frequency ν when the source, lens, and observer occupy fixed positions.…”

Section: Introductionmentioning

confidence: 99%

Femtolensing: Beyond the semiclassical approximation

Ulmer¹,

Goodman²

1995

ApJ

View full text Add to dashboard Cite

Femtolensing is a gravitational lensing effect in which the magnification is a function not only of the positions and sizes of the source and lens, but also of the wavelength of light. Femtolensing is the only known effect of (10 −13 − 10 −16 M ⊙ ) dark-matter objects and may possibly be detectable in cosmological gamma-ray burst spectra. We present a new and efficient algorithm for femtolensing calculations in general potentials. The physical-optics results presented here differ at low frequencies from the semi-classical approximation, in which the flux is attributed to a finite number of mutually coherent images. At higher frequencies, our results agree well with the semi-classical predictions. Applying our method to a point-mass lens with external shear, we find complex events that have structure at both large and small spectral resolution. In this way, we show that femtolensing may be observable for lenses up to 10 −11 solar masses, much larger than previously believed. Additionally, we discuss the possibility of a search for femtolensing of white dwarfs in the LMC at optical wavelengths.

show abstract

Mutual Interference and Structural Properties of Object Images in the Vicinity of the Gravitational Lens CUSP Point

Cited by 4 publications

References 1 publication

Wave Effects in the Gravitational Lensing of Gravitational Waves from Chirping Binaries

Wave Effects in the Gravitational Lensing of Gravitational Waves from Chirping Binaries

New constraints on primordial black holes abundance from femtolensing of gamma-ray bursts

Femtolensing: Beyond the semiclassical approximation

Contact Info

Product

Resources

About