| |
EI2GYB > ASTRO 03.09.21 12:00l 96 Lines 4248 Bytes #999 (0) @ WW
BID : 14046_EI2GYB
Read: GUEST
Subj: Astronomers Find Cosmic Boomerang in Coma Cluster Galaxy
Path: IW8PGT<LU4ECL<GB7CIP<EI2GYB
Sent: 210903/0957Z 14046@EI2GYB.DGL.IRL.EURO BPQ6.0.22
_ _ _ _
/ \ ___| |_ _ __ ___ | \ | | _____ _____
/ _ \ / __| __| '__/ _ \ | \| |/ _ \ \ /\ / / __|
/ ___ \\__ \ |_| | | (_) | | |\ | __/\ V V /\__ \
/_/ \_\___/\__|_| \___/ |_| \_|\___| \_/\_/ |___/
Astronomers Find Cosmic Boomerang in Coma Cluster Galaxy
Using data from the Atacama Large Millimeter Array (ALMA), the Combined Array
for Research in Millimeter-Wave Astronomy (CARMA) and the NASA/ESA Hubble
Space Telescope, astronomers have observed a cosmic boomerang effect -
molecular gas streams that are stripped away from a galaxy only to circle
back and return later - in the northwest quadrant of NGC 4921, a spiral
galaxy in the Coma cluster.
The observation offers new insights into the life cycle of galaxies and the
structural formations within galaxies, as traced by molecular gas.
The Coma cluster is a large group of galaxies approximately 330 million
light-years away in the northern constellation of Coma Berenices.
Also known as Abell 1656, the cluster is a great environment to study the
ram-pressure stripping - a process known to strip gas out of galaxies,
leaving them without the material needed to form new stars - at high resolution.
An excellent member of the cluster to study the effects of this process on
the dense interstellar medium is NGC 4921, a massive, nearly face-on spiral
galaxy.
"Astronomers are interested in studying how galaxies grow, live, and die,"
said Dr. William Cramer, a postdoctoral researcher at Arizona State University.
"Effects like ram pressure that can speed up the normal galaxy lifecycle are
very important to understand for this reason."
"Furthermore, the molecular gas in galaxies is the birthplace of new stars,
and therefore studying the effect of ram pressure on it is of paramount
importance."
Using data gathered by ALMA, Dr. Cramer and colleagues created a
high-resolution map of dense molecular gas in NGC 4921.
The map shows unusual structures that form in the ram pressure 'wind' - long
filaments of heavy gas connected to newly-forming stars.
This dense, heavy gas is thought to be more resistant to ram-pressure
stripping, perhaps due to magnetic fields holding it more firmly in place.
"When an external force like ram pressure disturbs a galaxy, it offers an
opportunity to learn about the internal forces that operate in galaxies,"
said Professor Jeffrey Kenney, a researcher at Yale University.
"The unusual filaments would not form without magnetic fields, so we also
learn about the importance of magnetic fields in galaxies from this ram
pressure interaction."
The ALMA data clearly show filaments of molecular gas connected to NGC
4921 - the filaments are, indeed, resisting.
But then the astronomer spotted something else - some of the previously-stripped
gas comes back.
"Instead of being thrown out never to return, some of this gas is moving like
a boomerang, being ejected but then circling and falling back to its source.
If this gas is recaptured into the galaxy, it can form new stars,"
Dr. Cramer said.
"The boomerang effect is significant for several reasons.
It provides hard evidence about the evolution of galaxies."
"It confirms a long-held theory about galaxy development; and it aids
astronomers trying to predict the birthrate of new stars."
"The interstellar medium of galaxies is complex, with many variables
that are hard to model."
"This observation is important because it shows that fallback of gas
can be detected and allows us to search more broadly to help characterize it."
The study will be published in the Astrophysical Journal.
____ __ ____ ___ _ _ ____ ____ ____ ____
( __)( )(___ \ / __)( \/ )( _ \ ( _ \( _ \/ ___)
) _) )( / __/( (_ \ ) / ) _ ( ) _ ( ) _ (\___ \
(____)(__)(____) \___/(__/ (____/ (____/(____/(____/
PART OF THE DONEGAL PACKET RADIO NETWORK
Packet: EI2GYB@EI2GYB.DGL.IRL.EURO
Email: EI2GYB@GMAIL.COM
+------------------------------------------------------------------------------+
Read previous mail | Read next mail
| |
