A cloudy mystery
It's
the mystery of the curiously dense cloud. And astronomers at the California
Institute of Technology (Caltech) are on the case. Near the crowded galactic
center, where billowing clouds of gas and dust cloak a supermassive black hole
three million times as massive as the sun -- a black hole whose gravity is
strong enough to grip stars that are whipping around it at thousands of
kilometers per second -- one particular cloud has baffled astronomers. Indeed,
the cloud, dubbed G0.253+0.016, defies the rules of star formation.
In
infrared images of the galactic center, the cloud -- which is 30 light-years
long -- appears as a bean-shaped silhouette against a bright backdrop of dust
and gas glowing in infrared light. The cloud's darkness means it is dense
enough to block light.
According
to conventional wisdom, clouds of gas that are this dense should clump up to
create pockets of even denser material that collapse due to their own gravity
and eventually form stars. One such gaseous region famed for its prodigious
star formation is the Orion Nebula. And yet, although the galactic-center cloud
is 25 times denser than Orion, only a few stars are being born there -- and
even then, they are small. In fact, the Caltech astronomers say, its
star-formation rate is 45 times lower than what astronomers might expect from
such a dense cloud.
"It's
a very dense cloud and it doesn't form any massive stars -- which is very
weird," says Jens Kauffmann, a senior postdoctoral scholar at Caltech.
In a
series of new observations, Kauffmann, along with Caltech postdoctoral scholar
Thushara Pillai and Qizhou Zhang of the Harvard-Smithsonian Center for
Astrophysics, have discovered why: not only does it lack the necessary clumps
of denser gas, but the cloud itself is swirling so fast that it can't settle
down to collapse into stars.
The
results, which show that star formation may be more complex than previously
thought and that the presence of dense gas does not automatically imply a
region where such formation occurs, may help astronomers better understand the
process.
The team presented their findings -- which have been recently
accepted for publication in the Astrophysical Journal Letters -- at the 221st meeting of the American
Astronomical Society in Long Beach, California.
To
determine whether the cloud contained clumps of denser gas, called dense cores,
the team used the Submillimeter Array (SMA), a collection of eight radio
telescopes on top of Mauna Kea in Hawaii. In one possible scenario, the cloud
does contain these dense cores, which are roughly 10 times denser than the rest
of the cloud, but strong magnetic fields or turbulence in the cloud disturbs
them, thus preventing them from turning into full-fledged stars.
However,
by observing the dust mixed into the cloud's gas and measuring N2H+ -- an ion that can only exist in
regions of high density and is therefore a marker of very dense gas -- the
astronomers found hardly any dense cores. "That was very surprising,"
Pillai says. "We expected to see a lot more dense gas."
Next,
the astronomers wanted to see if the cloud is being held together by its own
gravity -- or if it is swirling so fast that it is on the verge of flying
apart. If it is churning too fast, it can't form stars. Using the Combined
Array for Research in Millimeter-wave Astronomy (CARMA) -- a collection of 23
radio telescopes in eastern California run by a consortium of institutions, of
which Caltech is a member -- the astronomers measured the velocities of the gas
in the cloud and found that it is up to 10 times faster than is normally seen
in similar clouds. This particular cloud, the astronomers found, was barely
held together by its own gravity. In fact, it may soon fly apart.
The
CARMA data revealed yet another surprise: the cloud is full of silicon monoxide
(SiO), which is only present in clouds where streaming gas collides with and
smashes apart dust grains, releasing the molecule. Typically, clouds only
contain a smattering of the compound. It is usually observed when gas flowing
out from young stars plows back into the cloud from which the stars were born.
But the extensive amount of SiO in the galactic-center cloud suggests that it
may consist of two colliding clouds, whose impact sends shockwaves throughout
the galactic-center cloud. "To see such shocks on such large scales is
very surprising," Pillai says.
G0.253+0.016
may eventually be able to make stars, but to do so, the researchers say, it
will need to settle down so that it can build dense cores, a process that could
take several hundred thousand years. But during that time, the cloud will have
traveled a great distance around the galactic center, and it may crash into
other clouds or be yanked apart by the gravitational pull of the galactic
center. In such a disruptive environment, the cloud may never give birth to
stars.
The
findings also further muddle another mystery of the galactic center: the
presence of young star clusters. The Arches Cluster, for example, contains
about 150 bright, massive, young stars, which only live for a few million
years. Because that is too short an amount of time for the stars to have formed
elsewhere and migrated to the galactic center, they must have formed at their
current location. Astronomers thought this occurred in dense clouds like
G0.253+0.016. If not there, then where do the clusters come from?
The
astronomers' next step is to study similarly dense clouds around the galactic
center. The team has just completed a new survey with the SMA and is continuing
another with CARMA. This year, they will also use the Atacama Large Millimeter
Array (ALMA) in Chile's Atacama Desert -- the largest and most advanced
millimeter telescope in the world -- to continue their research program, which
the ALMA proposal committee has rated a top priority for 2013.
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Posted by Unknown
on Friday, January 11, 2013.
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