The main difference observed between ESO243-49HLX-1,
and say our old friend Cygnus X-1,
is that appears brighter and then
its spectrum has been shifted towards the redder end of the spectrum.
As astronomers watched over the next few years,
we saw repeated brightening of this source.
ESO243-49HLX-1 appeared to increase in brightness in a period of just over a year.
The spectrum of this source was seen to change in shape with brightness.
The time dependent emission of
ESO243-49HLX-1 is very similar to the behavior of X-ray binaries,
leading astronomers to believe that it is also a binary system.
This means that the black hole
ESO243-49HLX-1 may be actively consuming a star.
However, the cyclical nature of the outburst lead
some to suggest that this black hole may not be slowly
sipping on the surface of a star but may instead be
ripping off larger chunks before gobbling them up in feeding frenzies.
This would trigger outbursting behavior
observed that mirrors that of outbursts of X-ray binaries.
What could cause these periods of gloat and fasting?
The periodic feeding frenzies could be explained if
the binary system's orbit is elliptical instead of circular.
This means that the distance between the star and
the black hole changes periodically during the orbit.
When the star is at its furthest point from the black hole,
no mass will be transferred from the star to the black hole.
However, when the star is close to the black hole,
the gravitational pull of the black hole will increase, allowing
the black hole to attract large amounts of material from the star to the accretion disc.
This famine and bloat cycle has been suggested as a way to create
the regular outburst witnessed from ESO243-49HXL-1.
Further studies have indicated that this black hole weighs in at
about 10,000 times the mass of our Sun and that
resides in the center of a dwarf galaxy that has been stripped
and squashed during its interactions with ESO243-49.
These interactions may have triggered the formation of the star now feeding
the black hole and may have pushed it into an elliptical orbit that now feeds the beast.
The cigar shaped galaxy, M82,
is the home of another candidate intermediate mass black hole.
M82 is a starburst galaxy where stars formed at a rate much higher than our own galaxy.
The X-ray inset shows us a bright X-ray source
named X-1, which is possibly an intermediate-mass black hole.
M82 X-1 lies outside the galaxy's core.
It was first detected in 1978
when it piqued the interest of astronomers due to its strange brightness.
The reason that this thought source was thought to be so strangely bright,
is that it emits light at a much greater rate than we
would expect to see if the source was a stellar mass black hole.
The luminosity of M82 X-1 could have been explained by
a supermassive black hole and yet supermassive black holes are found in galaxy centers,
while M82 X-1 does not lie in the center of its host galaxy.
This left astronomers with two options.
The first option is that this black hole lies in the intermediate mass black hole range.
If this was the case,
it could explain the luminosity of M82 X-1.
However, an alternative theory emerged.
The idea that this may be a stellar mass black hole undergoing a feeding frenzy.
If it is a stellar mass black hole
then it is creating a previously on observed gigantic rates.
As more observations have been made of this source,
the mass estimate of M82 X-1 has bounced
between stellar mass and intermediate mass over the last 40 years.
Today, evidence seems to be mounting in support of an intermediate mass black hole with
a mass estimated in the range of 400 to 100 thousand solar masses.
It's interesting to note however,
that M82 X-1's close neighbor,
M82 X-2, has recently shown just how extreme accreters can get.
In 2014, a team working with data from New Star Chandra and Swift Satellites,
discovered that a previously observed X-ray source,
M82 X-2, is in fact a class of neutron stars known as a pulsar.
A pulsar is a rotating neutron star that shoots jets of emission from its poles.
These jets sweep across all field of view as the star rotates like a lighthouse beam,
sweeps over the rocks and out to sea.
The striking thing about this neutron star is that it is
100 times brighter than theory predicts it could be.
This means that M82 X-2 is one of the most extreme objects in our galaxy,
and it can be used to help us understand how
supermassive black holes could grow so quickly in the early universe.
Enough about neutron stars though.
Let's get back to intermediate-mass black holes.
The next candidate intermediate-mass black hole is XJ1417+52.
This black hole has a mass that lies at the upper boundary for
intermediate-mass black holes approaching the range of the supermassive black holes.
Omega Centauri is a globular cluster found in the constellation of Centaurus.
It is located almost 16,000 light years
away and it's the largest globular cluster in the Milky Way.
This star cluster may be home to
our final example of a candidate intermediate-mass black hole.
Unlike the other candidate intermediate-mass black holes,
this black hole was not identified through its X-ray emission.
Most likely, this black hole is not actively
feeding since there is no substantial food source nearby.
The candidate intermediate mass black hole in Omega Centauri within feed,
I observing the motions of stars using optical telescopes.
These stars in the globular cluster move around randomly like a swarm of bees.
The speeds of these stars are related to the total mass of the star cluster.
From the observations of the star's motion,
the mass, the center of the cluster can be inferred.
Different observations suggest that black hole with a mass in the range of 10,000
to 15,000 solar masses lies in the center of Omega Centauri.
