A new look at microlensing
Through a Hubble Space Telescope analysis of stars that have undergone
gravitational microlensing, astronomers have collected strong evidence
that microlensing events are caused by compact dark matter in the halo
of the Milky Way. The findings were presented Monday by Lab researchers
Cailin Nelson and Kem Cook on behalf of the Massive Compact Halo Objects
(MACHO) collaboration during the annual meeting of the American Astronomical
Society in San Diego.
Astronomers believe the dark matter in the Milky Way is distributed in
a spherical halo of matter, which extends more than 10 times farther than
the disk of visible stars. Some of this matter may be in one of many primarily
baryonic forms including planets, brown dwarfs, very old low-mass stars,
neutron stars and low-mass black holes. They are collectively known as
MACHOs.
Though MACHOs emit some light, their level of emission is below present-day
detection thresholds. They can be found indirectly by noting the gravitational
signature they produce as they interact with other visible objects. One
such signature is microlensing. In a microlensing event, a MACHO passes
through an observer’s line of sight to an ordinary, luminous star.
The gravitational presence of the MACHO bends the light from the star,
and, acting like a lens, causes a temporary apparent increase in the brightness
of the star. The brightened star in a microlensing event is called the
source star.
The MACHO project has been monitoring the sky — through the use of
the 1.27-meter telescope at Mount Stromlo Observatory in Australia —
for microlensing events in a line of sight toward a nearby galaxy, the
Large Magellanic Cloud (LMC), for eight years. The LMC provides a convenient
backdrop of source stars. Earlier MACHO project results show that MACHOs
can account for about 20 percent mass in the Milky Way halo and that MACHO
mass is most likely between 0.15 and 0.9 times the mass of the Sun.
Some astronomers, however, have remained skeptical that the microlensing
events are actually produced by MACHOs in the halo of the Milky Way, instead
speculating that it is faint stars in the LMC lensing other stars in the
LMC, which cause microlensing events. To make these non-dark matter theories
for microlensing viable, these models also must include adjustments to
the generally accepted structure of the LMC.
These adjustments require different arrangements of the source stars.
If dark matter causes the microlensing events, the source stars will be
randomly distributed in the LMC. Conversely, if normal stars in the LMC
cause the microlensing events, the source stars will be found toward the
far side of the LMC. This subtle effect can be detected by taking Hubble
Space Telescope images of the microlensing source stars. The MACHO project
recently has completed this analysis.
"Our analysis has determined that it is very unlikely that microlensing
is due to some strange population of source stars behind the LMC,"
said Nelson, a University of California at Berkeley graduate student,
who works at Livermore’s Institute for Geophysics and Planetary Physics.
"We can also say that it is somewhat unlikely that microlensing is
due to any sort of spherical distribution of stars in a halo around the
LMC. The most likely explanation remains that microlensing events are
caused by dark matter MACHOs in the halo of the Milky Way."
It is generally impossible to measure the characteristics needed from
ground-based data to determine the arrangement of source stars. The ground-based
MACHO images taken on the Mount Stromlo Observatory are very crowded,
causing several nearby stars in the LMC to blend together and appear as
one blended "object" in the ground-based image. Only one of
the stars in the microlensed object is actually lensed and thus the ground-based
data provides little detail about the properties of the actual source
star. To eliminate this confusion, Hubble Space Telescope data of the
area surrounding each microlensing event was obtained. Using a technique
known as difference-image analysis, it was then possible to identify the
source star of each microlensing event.
Using the brightness and color of the source stars, the LLNL team determined
the distribution of source stars in the LMC. They found no evidence that
the source stars are not randomly distributed in the LMC.
Additionally, this analysis ruled out with high confidence (99 percent)
any model in which all of the source stars are located behind the LMC
disk. It also ruled out with some confidence (about 80 percent) models
in which two thirds of the source stars were located behind the LMC disk.
Astronomers have long known that most of the matter in the universe is
invisible. This dark matter gives off no light, yet can be detected through
its gravitational interaction with other luminous forms of matter such
as stars and galaxies. The dark matter pervades all space, both within
galaxies and in the vast "empty" space between them.
A significant component of the dark matter must be made up of some sort
of exotic elementary particle that has yet to be detected. However, a
small fraction of the dark matter consists of baryons. Studies show that
our universe holds several times more baryons than we can count as visible
light in stars and galaxies.
The MACHO collaboration consists of scientists from the Lab (Kem Cook,
Andrew Drake, Stuart Marshall, Cailin Nelson and Piotr Popowski); the
University of Pennsylvania; the Australian National Supercomputing Facility;
STScI; the Mount Stromlo Observatory; Bell Labs; University of Notre Dame;
UC Santa Cruz; UC San Diego; Universidad Catolica; University of Washington;
the European Southern Observatory; the University of Oxford; and McMaster
University.