6.3 Exploitation of Time Delays
The occurrence of time delays among multiple images of a lensed source
can provide unique opportunities to study transient phenomena. For
instance, were a supernova to go off in a multiply-imaged region of an
arc-galaxy, the explosion will be seen three or more times with delays
(Kovner &
Paczynski 1988).
If a reasonable estimate of the
time delay is available (say from a model), one could wait and observe
one of the later incarnations of the event in much greater detail than
would be possible without prior warning. (However, this will not
provide a measurement of H0 as the cluster potential
is unlikely to
be understood well enough.) The same principle could be used with any
unusual event in the multiply-imaged quasars, e.g. transient flaring of
the optical or X-ray emission, or ejection of a radio VLBI blob.
The BATSE experiment on the Compton Gamma Ray Observatory
(Meegan et
al. 1992)
has shown that most gamma-ray bursts are isotropically
distributed on the sky and have non-Euclidean source counts, which
suggests that they lie at cosmological distances (e.g.
Prilutski & Usov
1975,
Mao & Paczynski
1992).
If so, gamma-ray bursts
constitute a fairly homogeneous population of near point sources with
(model-dependent) angular sizes ~ 10-20 radians. Gamma-ray
telescopes have only primitive angular resolving power, but sub
millisecond temporal resolution, and so this hypothesis can be tested
by seeking multiple bursts from the same source separated in time by
~ 10-5 (M / M) s where M is the lens mass
(Paczynski
1986b,
1987b).
Known galaxies will create repeating bursts with
median time delays ~ 1 month with a probability ~ 10-3
(Mao 1992),
and examples ought to be seen after ~ 3 yr of full
operation of BATSE. Microlensing by individual stars will probably
not be resolvable, but a cosmologically significant density of
compact masses with M 100M could be detected. Using
the observed time delays and magnification ratios, the masses of the
individual lenses could be determined with good accuracy
(Narayan &
Wallington 1992).
Interestingly, for a lens with mass
1018 g, the Fresnel length will be smaller than the Einstein
radius and energy-dependent diffraction effects are predicted
(Bliokh &
Minakov 1975,
Gould 1992).
Multiply-imaged quasars provide unique opportunities to probe the
intervening intergalactic medium between us and the source. Since
the geometry of the two ray-paths is known, the presence or absence
of common absorption lines in the multiple spectra leads to powerful
constraints on the transverse sizes of Lyman- clouds and
metal-line systems.
(Weymann et
al. 1979,
Krolik & Kwan 1979,
Young et
al. 1981c,
Weymann & Foltz
1983,
Foltz et
al. 1984,
Thomas & Webster
1990,
Steidel &
Sargent 1990,
Smette et
al. 1992).
Sizes of 5-25 kpc have been deduced from Lyman- absorption lines
observed in Q0957+561 and Q2345+007. Conversely, the redshift
distribution of the absorption systems in the images can be used as
an argument for, or against, multiple imaging
(Duncan 1991,
Steidel &
Sargent 1991).
For most models of the clouds responsible for the Lyman-
forest, no significant gravitational lensing is expected by the
clouds themselves
(Ikeuchi &
Turner 1991).