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MACHO Detection from Measurements of Gravitational Deflection

Published online by Cambridge University Press:  25 May 2016

Kouji Ohnishi ,
Mizuhiko Hosokawa  and
Toshio Fukushima
Kouji Ohnishi
Affiliation:
Nagano National College of Technology Nagano 381-8550, Japan
Mizuhiko Hosokawa
Affiliation:
Communications Research Laboratory 4-2-1 Nukui-kita, Koganei, Tokyo 184, Japan
Toshio Fukushima
Affiliation:
National Astronomical Observatory 2-21-1,Ohsawa, Mitaka, Tokyo 181, Japan

Extract

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The observed positions of quasars are fluctuated due to the gravitational lensing of the matters in our galaxy. The magnitude of fluctuation due to stars and MACHOs is of the order of a few micro-arc second (μas) ∼ 10 μas and its time scale is of the order of a few years ∼ hundreds years (Hosokawa et al. 1997). Such fluctuation will reflects the nature of the constituents, both visible and invisible, of our galaxy.

Type
IV. Structure Formation and Dark Matter
Information
Symposium - International Astronomical Union , Volume 183: Cosmological Parameters and the Evolution of the Universe , 1999 , pp. 261
Copyright
Copyright © Kluwer 1999 

References

Hosokawa, M., Ohnishi, K., & Fukushima, , 1997, AJ, 114, 1508 CrossRefGoogle Scholar
Sasao, T., et.al., 1994, VLBI Technology, ed. Sasao, T., Manabe, S., Kameya, O. & Inoue, M., (Terra Scientific Publ. Co.), 254 Google Scholar