Optical BVI imaging and H I synthesis observations of the dwarf irregular Galaxy ESO 364-G029

M. B. N. Kouwenhoven; M. Bureau; S. Kim; P. T. de Zeeuw

doi:doi:10.1051/0004-6361:20077531

Free access

Issue		A&A Volume 470, Number 1, July IV 2007


Page(s)		123 - 135
Section		Extragalactic astronomy
DOI		http://dx.doi.org/10.1051/0004-6361:20077531

A&A 470, 123-135 (2007)
DOI: 10.1051/0004-6361:20077531

Optical BVI imaging and H I synthesis observations of the dwarf irregular Galaxy ESO 364-G029

M. B. N. Kouwenhoven^{1, 2, 3}, M. Bureau⁴, S. Kim⁵, and P. T. de Zeeuw²

¹ Department of Physics and Astrophysics, University of Sheffield, Hicks Building, Hounsfield Road, Sheffield S3 7RH, UK
    e-mail: t.kouwenhoven@sheffield.ac.uk
² Sterrewacht Leiden, Leiden University, Niels Bohrweg 2, 2333 CA Leiden, The Netherlands
    e-mail: tim@strw.leidenuniv.nl
³ Astronomical Institute Anton Pannekoek, Kruislaan 403, 1098 SJ, Amsterdam, The Netherlands
⁴ Department of Physics, University of Oxford, Denys Wilkinson Building, Keble Road, Oxford OX1 3RH, UK
    e-mail: bureau@astro.ox.ac.uk
⁵ Astronomy & Space Science Department, Sejong University, 98 Kwangjin-gu, Kunja-dong, Seoul 143-747, Korea
    e-mail: sek@sejong.ac.kr

(Received 23 March 2007 / Accepted 16 April 2007 )

Abstract
As part of an effort to enlarge the number of well-studied Magellanic-type galaxies, we obtained broadband optical imaging and neutral hydrogen radio synthesis observations of the dwarf irregular galaxy ESO 364-G029 . The optical morphology characteristically shows a bar-like main body with a one-sided spiral arm, an approximately exponential light distribution, and offset photometric and kinematic centers. The $\ion{H}{i}$ distribution is mildly asymmetric and, although slightly offset from the photometric center, roughly follows the optical brightness distribution, extending to over 1.2 Holmberg radii (where $\mu_B=26.5$ mag arcsec^-2). In particular, the highest $\ion{H}{i}$ column densities closely follow the bar, one-arm spiral, and a third optical extension. The rotation is solid-body in the inner parts but flattens outside of the optical extent. The total $\ion{H}{i}$ flux $F_\ion{H}{i}=23.1$ $\pm$ 1.2 Jy km s^-1, yielding a total $\ion{H}{i}$ mass $M_\ion{H}{i}=(6.4\pm1.7)$ $\times$ 10⁸ ${M}_\odot$ (for a distance D=10.8 $\pm$ 1.4 Mpc) and a total $\ion{H}{i}$ mass-to-blue-luminosity ratio $M_\ion{H}{i}/L_B=(0.96\pm0.14)$ ${M}_\odot/ {L}_{B,\odot}$ (distance independent). The $\ion{H}{i}$ data suggest a very complex small-scale $\ion{H}{i}$ structure, with evidence of large shells and/or holes, but deeper observations are required for a detailed study. Follow-up observations are also desirable for a proper comparison with the Large Magellanic Cloud, where despite an optical morphology very similar to ESO 364-G029 the $\ion{H}{i}$ bears little resemblance to the optical.

Key words: galaxies: individual: ESO 364-G029 -- galaxies: irregular -- galaxies: photometry -- galaxies: kinematics and dynamics -- galaxies: structure -- galaxies: ISM

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