ePrints@IIScePrints@IISc Home | About | Browse | Latest Additions | Advanced Search | Contact | Help

A radio study of the superwind galaxy NGC 1482

Hota, Ananda and Saikia, DJ (2005) A radio study of the superwind galaxy NGC 1482. In: Monthly Notices of the Royal Astronomical Society, 356 (3). pp. 998-1008.

[img] PDF
A_radio_study_of_the_superwind_galaxy_NGC_1482.pdf
Restricted to Registered users only

Download (461Kb) | Request a copy

Abstract

We present multifrequency radio continuum as well as H i observations of the superwind galaxy NGC 1482, with both the Giant Metrewave Radio Telescope (GMRT) and the Very Large Array (VLA). This galaxy has a remarkable hourglass-shaped optical emission-line outflow as well as bipolar soft X-ray bubbles on opposite sides of the galactic disc. The low-frequency, lower-resolution radio observations show a smooth structure. From the non-thermal emission, we estimate the available energy in supernovae, and examine whether this would be adequate to drive the observed superwind outflow. The high-frequency, high-resolution radio image of the central starburst region located at the base of the superwind bi-cone shows one prominent peak and more extended emission with substructure. This image has been compared with the infrared, optical red continuum, H\alpha, and soft and hard X-ray images from Chandra to understand the nature and relationship of the various features seen at different wavelengths. The peak of the infrared emission is the only feature that is coincident with the prominent radio peak, and possibly defines the centre of the galaxy. The $H_I$ observations with the GMRT show two blobs of emission on opposite sides of the central region. These are rotating about the centre of the galaxy and are located at \sim2.4 kpc from it. In addition, these observations also reveal a multicomponent $H_I$ absorption profile against the central region of the radio source, with a total width of \sim250 km s-1. The extreme blue- and redshifted absorption components are at 1688 and 1942 $km s^{-1}$, respectively, while the peak absorption is at 1836 $km s^{-1}$. This is consistent with the heliocentric systemic velocity of 1850 \pm 20 $km s^{-1}$, estimated from a variety of observations. We discuss possible implications of these results.

Item Type: Journal Article
Additional Information: Copyright of this article belongs to Blackwell.
Department/Centre: Division of Physical & Mathematical Sciences > Joint Astronomy Programme
Date Deposited: 12 Feb 2007
Last Modified: 19 Sep 2010 04:34
URI: http://eprints.iisc.ernet.in/id/eprint/9419

Actions (login required)

View Item View Item