Molecular gas in Arp 94: implications for intergalactic star formation
Metadata
Show full item recordEditorial
Elsevier B.V.
Materia
Galaxies Star formation Molecular gas Arp 94
Date
2006Referencia bibliográfica
Lisenfeld, U.; et al. Molecular gas in Arp 94: implications for intergalactic star formation. New Astronomy Reviews, 51(1-2): 63-66 (2007). [http://hdl.handle.net/10481/28408]
Abstract
We present CO(1-0) observations of the interacting galaxy system Arp 94, which
contains the Seyfert galaxies NGC 3227 and NGC 3226 as well as the star-forming
candidate dwarf galaxy J1023+1952. We mapped the CO distribution in J1023+1952
with the IRAM 30m telescope and found molecular gas across the entire extent of
the neutral hydrogen cloud – an area of about 9 by 6 kpc. The region where star
formation (SF) takes place is restricted to a much smaller (∼ 1.5 by 3 kpc) region
in the south where the narrow line width of the CO shows that the molecular gas
is dynamically cold. Neither the molecular nor the total gas surface density in the
SF region are significantly higher than in the rest of the object suggesting that an
external trigger is causing the SF. The fact that CO is abundant and apparently
a good tracer for the molecular gas in J1023+1952 indicates that its metallicity is
relatively high and argues for a tidal origin of this object.