|Statement||edited by John Menzies and Penny D. Sackett.|
|Series||Astronomical Society of the Pacific conference series -- vol.239|
|Contributions||Menzies, J. W., Sackett, Penny D., Astronomical Society of the Pacific.|
|The Physical Object|
|Pagination||xiv, 401p. :|
|Number of Pages||401|
Menzies, J. W. (Editor) , ASP Conf. Proc. Ser. ‘Microlensing , A New Era of Microlensing Astrophysics’ Google Scholar. In a article, Gould et al. derived a planet frequency beyond the snow line from microlensing that was a factor 7 larger than the one derived from radial velocity studies for planets with much shorter periods, from 2 to days. This difference was consistent with the gradient derived from radial velocity results when these were Cited by: 8. We analyze the data of the gravitational microlensing survey carried out by the Microlensing Observations in Astrophysics (MOA) group during toward the Galactic bulge (GB). Our observations are designed to detect efficient high-magnification events with faint source stars and short-timescale events, by increasing the sampling rate up to ~6 Cited by: Journal/Book Title/Conference. Can Gravitational Waves Be Detected in Quasar Microlensing? Publication Date. Comments. self-archived. Recommended Citation. Can gravitational waves be detected in quasar microlensing? Shane L. Larson and Rudolph Schild : astro-ph/ This document is currently not available : Shane L. Larson, Rudolph Schild.
Abstract: We propose a genuine, 3-dimensional offset between the "bar" and the disc components of the LMC, where the LMC's off-centered "bar" is an unvirialized structure slightly misaligned with, and offset from, the plane of the LMC disk perhaps due to recent tidal interactions of the LMC with the SMC and with the Galaxy (Zhao & Evans ). In , Robert J. Nemiroff predicted the likelihood of microlensing and calculated basic microlensing induced light curves for several possible lens-source configurations in his thesis.  In Mao and Paczyński suggested that microlensing might be used to find binary companions to stars, and in Gould and Loeb demonstrated that. Gravitational microlensing occurs when a foreground star happens to pass very close to our line of sight to a more distant background star. The foreground star acts as a lens, splitting the light from the source star into two images, which are typically unresolved. However, these images are also magnified, by an amount that depends on the angular lens-source . Using gravitational microlensing technique, an international group of astronomers has found a new substellar system whose composition remains a puzzle. The newly detected system, designated MOA.
Abstract. Since the first discoveries (Aubourg et al. ) (Alcock et al. ) (Udalski et al. ), hundreds of microlensing effects have been detected in the direction of the galactic bulge together with a handfull of events towards the EROS microlensing searches in the LMC and (more recently) SMC directions are sensitive to the component of the galactic dark Author: M. Moniez. Gravitational Microlensing: Searches and Results As mentioned in the previous lecture, we are able to resolve the rings and arcs produced by very massive gravitational lenses: entire galaxies, and clusters of galaxies. The Einstein ring radius of a single star is tiny: about arcseconds, much too small to be seen by telescopes on the. The first gravitational microlensing events were discovered in by MACHO1, EROS2, and OGLE3, and by now, ~ microlensing events have been observed4,5. The first microlensing planet discovery was announced in by MOA and OGLE6. The microlensing signals of planets are distinctive and diagnostic. Abstract. We consider the influence of microlensing on different spectral bands of lensed QSOs. We assumed that the emitting X-ray, ultraviolet (UV) and optical regions are different in size, but that the continuum emission in these Cited by: