A Radio Perspective on the Wet Merger Remnant NGC 34

Details A Radio Perspective on the Wet Merger Remnant NGC 34 A Radio Perspective on the Wet Merger Remnant NGC 34

Jan 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21541027x&link_type=abstract

American Astronomical Society, AAS Meeting #215, #410.27; Bulletin of the American Astronomical Society, Vol. 42, p.239

Astronomy and Astrophysics

Astronomy

Scientific paper

We present the VLA observations of the neutral hydrogen content and the radio continuum of NGC 34. This object is an ideal candidate to study the fate of gas in mergers, since, as shown by an optical study done by Schweizer & Seitzer (2007), it is a gas-rich (wet) merger remnant of two galaxies of unequal mass hosting a strong central starburst and a weak AGN. We detect HI emission from both tidal tails and nearby galaxies, suggesting NGC 34 is actually part of a gas-rich group and it might be interacting with one of its companions. The kinematics of the gas suggest this remnant is forming an outer disk of neutral hydrogen. We also detect broad HI absorption (514 km/s) at velocities that are both blueshifted and redshifted with respect to the systemic velocity, which could be explained by the motions of the tidal tails or by the presence of a circumnuclear disk. In addition, we present radio continuum images that show both nuclear (61.2 mJy) and extra-nuclear emission (24.6 mJy). This extra-nuclear component is very diffuse and in the shape of radio lobes, spanning 387 kpc. This emission could originate from a starburst-driven superwind or can be a signature of an AGN that has turned off. We discuss the possible scenarios that explain our observations, and what they tell us about the location of the gas and the future evolution of NGC 34.

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