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For refcode 1997AJ....113.2006E:
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Copyright by American Astronomical Society. Reproduced by permission
1997AJ....113.2006E THE IONIZED GAS AND RADIO HALO OF NGC 3432 (ARP 206) JAYANNE ENGLISH AND JUDITH A. IRWIN Queen's University, Department of Physics, Kingston, Ontario, K7L 3N6, Canada, Electronic mail: english@astro.queensu.ca; irwin@astro.queensu.ca Received 1996 June 28; revised 1997 February 21 ABSTRACT VLA data of the interacting galaxy, NGC 3432, display a radio continuum halo, with a maximum extent of 5.3 kpc in projection above the plane, containing considerable substructure and discrete radio continuum "spurs.'' The detection of high latitude H{alpha} emission, either in the form of an extended diffuse layer (DIG) or in discrete features, is often assumed to independently confirm the correlation of disk-halo interactions and underlying star formation. However, the possibly extra- planar optical features in our narrowband H{alpha} CCD images, acquired at Observatoire Mont Megantic, contain a significant stellar component suggesting they are not gaseous debris resulting from a "blow out" by star formation activity in the disk but rather are tidal features. Although the inclination (790) of NGC 3432 hinders our ability to detect a DIG halo surrounding this galaxy with these data, we can confirm that it has a lower star formation rate than the Milky Way. Hence it is an interesting counter-example to the notion that pervasive radio halos exist in galaxies with high star formation rates. We suggest that the interaction between NGC 3432 and UGC 5983, rather than disk-halo outflow in NGC 3432, is responsible for any extra-planar features as well as the extended radio continuum halo.
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