All Figures

$\begin{figure} \par\includegraphics[width=7.25cm,clip]{7531_1.eps} \end{figure}$ Figure 1: Optical image of ESO 364-G029 from the Digitized Sky Survey (DSS); cf. our $\it BVI$ images in Fig. 2.
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In the text

$\begin{figure} \par\includegraphics[width=5.25cm,clip]{7531_2a.eps}\hspace*{3mm}... ...eps}\hspace*{3mm} \includegraphics[width=5.25cm,clip]{7531_2c.eps}\end{figure}$ Figure 2: Logarithmic grayscale images of ESO 364-G029 in the Cousins B ( left), V ( middle) and I ( right) filters. The central bar and one spiral arm characterize ESO 364-G029 as a Magellanic-type dwarf galaxy.
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In the text

$\begin{figure} \par\includegraphics[width=6.4cm,clip]{7531_3.eps} \end{figure}$ Figure 3: The azimuthally-averaged surface brightness profiles of ESO 364-G029 in the B band ( solid curve), the V band ( dashed curve) and the I band ( dotted curve). The error bars indicate the $1\sigma$ formal errors. Systematic errors due to the irregular morphology of ESO 364-G029 are probably much larger. The dotted lines indicate the semi-major axis of ESO 364-G029 at the B=25 and 26.5 mag arcsec^-2 isophotes, respectively: $R_{25}= 1\hbox {$.\mkern -4mu^\prime $ }27$ $\pm$ $0\hbox {$.\mkern -4mu^\prime $ }03$ and $R_{\rm Ho}= 2\hbox {$.\mkern -4mu^\prime $ }30$ $\pm$ $0\hbox {$.\mkern -4mu^\prime $ }08$ .
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{7531_4.eps} \end{figure}$ Figure 4: Ellipticity $\epsilon$ ( top) and position angle PA ( bottom) profiles of ESO 364-G029, derived with the azimuthally-averaged B surface brightness profile shown in Fig. 3. Due to the irregular morphology of ESO 364-G029 it was not possible to successfully fit ellipses at radii larger than $83\hbox {$^{\prime \prime }$ }$ . $\epsilon$ and PA are assumed to be constant for radii larger than this value. The error bars indicate $1\sigma$ formal errors. Systematic errors due to the irregular morphology of ESO 364-G029 are probably much larger. The dotted lines in both panels indicate the ellipticity and position angle at radii R₂₅ and $R_{\rm Ho}$ .
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In the text

$\begin{figure} \par\includegraphics[width=6.55cm,clip]{7531_5.eps} \end{figure}$ Figure 5: Color profiles of ESO 364-G029, derived from the azimuthally-averaged surface brightness profiles shown in Fig. 3: B-V ( solid curve), V-I ( dashed curve) and B-I ( dotted curve). The error bars indicate the $1\sigma$ formal errors. Systematic errors due to the irregular morphology of ESO 364-G029 are probably much larger. Vertical dotted lines are plotted at radii R₂₅ and $R_{\rm Ho}$ .
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In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{7531_6.eps} \end{figure}$ Figure 6: H I channel maps of ESO 364-G029 for datacube UL (see Table 3). Each map is the average of 5 channels to increase the sensitivity (8.25 km s^-1 per map). Contour levels are at 3, 6, 9 and 12 times the rms noise in each map (1.2 mJy beam). The heliocentric velocity range of each map is indicated in the top-left corner. The synthesized beam is $21\hbox {$^{\prime \prime }$ }$ $\times$ $10\hbox {$^{\prime \prime }$ }$ with a position angle of $30\hbox {$^\circ $ }$ , and is indicated in the bottom-right panel.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{7531_7.eps} \end{figure}$ Figure 7: The global H I profile of ESO 364-G029 ( solid line), obtained from datacube NH by integrating the individual channel maps over the area containing emission. The total H I flux is $F_H {\sc i}=23.1$ $\pm$ 1.2 Jy km s^-1. The HIPASS global profile summed over a $40\hbox {$^\prime $ }$ $\times$ $40\hbox {$^\prime $ }$ area is overplotted ( dotted line). For clarity, the error bars for our ATCA data are only plotted for each fourth channel.
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In the text

$\begin{figure} \par\includegraphics[width=7.25cm,clip]{7531_8a.eps}\vspace*{3mm} \includegraphics[width=7cm,clip]{7531_8b.eps} \end{figure}$ Figure 8: Total H I maps of ESO 364-G029 for the low sensitivity (high resolution) datacubes. Top: UL isodensity contours overlaid on a grayscale representation. The contours represent 1, 2 and 4 times the faintest contour of 50 mJy beam^-1 km s^-1 or 2.65 $\times$ 10²⁰ cm^-2. Bottom: NL contours overlaid on a DSS image. The contours represent 1, 5, 10, 15, 20, 25 and 30 times the faintest contour of 80 mJy beam^-1 km s^-1 or 0.4 $\times$ 10²⁰ cm^-2. The contours generally increase toward the center and the synthesized beam is indicated in the bottom-left corner of each map.
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In the text

$\begin{figure} \par\includegraphics[width=7.25cm,clip]{7531_9a.eps}\vspace*{3mm} \includegraphics[width=7.25cm,clip]{7531_9b.eps} \end{figure}$ Figure 9: Same as Fig. 8 but for the velocity fields of ESO 364-G029. The isovelocity contours increase toward the North-East and cover the velocity range 750-820 km s^-1 in both panels. The contours are spaced by 10 km s^-1 ( top) and 5 km s^-1 ( bottom).
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In the text

$\begin{figure} \par\includegraphics[width=7.25cm,clip]{7531_10a.eps}\vspace*{3mm} \includegraphics[width=7.25cm,clip]{7531_10b.eps} \end{figure}$ Figure 10: Same as Fig. 8 but for the velocity dispersion fields of ESO 364-G029. The contours generally increase toward the center and represent 2 and 6 km s^-1 ( top) (unreliable) and 8 and 12 km s^-1 ( bottom).
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{7531_11.eps}\end{figure}$ Figure 11: The rotation curve of ESO 364-G029 as derived from the tilted-ring model described in the text, overlaid on a grayscale of the major-axis position-velocity diagram (datacube NL; beam size $58\hbox {$^{\prime \prime }$ }$ $\times$ $38\hbox {$^{\prime \prime }$ }$ ). The data points at radii larger than $2\hbox {$.\mkern -4mu^\prime $ }3$ are obtained from datacube NH (beam size $132\hbox {$^{\prime \prime }$ }$ $\times$ $70\hbox {$^{\prime \prime }$ }$ ), which has a higher sensitivity. The solid curve shows the fit to the whole velocity field, while the crosses show the fit to the approaching side ( left) and receding side ( right) of the galaxy only. Contour levels are overlaid at 7.5, 20, 40, 60 and 80 mJy beam^-1. Rotational velocities are not corrected for the uncertain inclination. For an inclination $i=70\hbox{$.\!\!^\circ$ }5$ (HyperLEDA), the rotation curve must be scaled up by $6\%$ .
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In the text

$\begin{figure} \par\includegraphics[width=7.25cm,clip]{7531_1.eps} \end{figure}$	Figure 1: Optical image of ESO 364-G029 from the Digitized Sky Survey (DSS); cf. our $\it BVI$ images in Fig. 2.
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$\begin{figure} \par\includegraphics[width=5.25cm,clip]{7531_2a.eps}\hspace{3mm}... ...eps}\hspace{3mm} \includegraphics[width=5.25cm,clip]{7531_2c.eps}\end{figure}$	Figure 2: Logarithmic grayscale images of ESO 364-G029 in the Cousins B ( left), V ( middle) and I ( right) filters. The central bar and one spiral arm characterize ESO 364-G029 as a Magellanic-type dwarf galaxy.
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$\begin{figure} \par\includegraphics[width=7.25cm,clip]{7531_9a.eps}\vspace*{3mm} \includegraphics[width=7.25cm,clip]{7531_9b.eps} \end{figure}$	Figure 9: Same as Fig. 8 but for the velocity fields of ESO 364-G029. The isovelocity contours increase toward the North-East and cover the velocity range 750-820 km s^-1 in both panels. The contours are spaced by 10 km s^-1 ( top) and 5 km s^-1 ( bottom).
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$\begin{figure} \par\includegraphics[width=7.25cm,clip]{7531_10a.eps}\vspace*{3mm} \includegraphics[width=7.25cm,clip]{7531_10b.eps} \end{figure}$	Figure 10: Same as Fig. 8 but for the velocity dispersion fields of ESO 364-G029. The contours generally increase toward the center and represent 2 and 6 km s^-1 ( top) (unreliable) and 8 and 12 km s^-1 ( bottom).
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