ESO340-G09     20:17:20.2    $-$38:40:29        7.0$\pm$1      9.0           160.3       14.52$\pm$0.27    $\cdots$          2546                       98.0
  ESO358-G26     03:35:30.8    $-$34:26:49     $-$1.6$\pm$2      4.2           153.1       12.90$\pm$0.40      +1.19           1660                       84.0
  ESO358-G29     03:36:31.4    $-$35:17:38     $-$2.0$\pm$1      3.9           153.1       12.47$\pm$0.18      +1.45           1740                      139.2
  ESO416-G25     02:48:41.3    $-$31:32:09        3.2$\pm$1      6.0           141.3       14.68$\pm$0.25      +1.38           4992                       31.0
  ESO460-G31     19:44:21.2    $-$27:24:22        4.8$\pm$1      9.5           154.9       15.15$\pm$0.21    $\cdots$       5352$^{1)}$                   92.0
  ESO487-G02     05:21:48.6    $-$23:48:45        3.9$\pm$1      7.5           199.5       13.62$\pm$0.26      +1.35        2088$^{1)}$                   60.0
  ESO531-G22     21:40:29.5    $-$26:31:40        4.5$\pm$1      8.7           154.2       13.94$\pm$0.35    $\cdots$       3639$^{1)}$                    8.0
  ESO555-G36     06:07:41.5    $-$19:54:54        5.5$\pm$1      11.5          139.6       15.60$\pm$0.58      +1.62         $\cdots$                    146.0
  ESO564-G27     09:11:54.3    $-$20:07:04        6.1$\pm$1      14.0          278.6       14.39$\pm$0.90      +1.36           2178                      168.0
  ------------ -------------- -------------- -------------- -------------- -------------- ---------------- ------------- ----------------- -------------------

$^{1)}$ Heliocentric radial velocities from Mathewson et al. (1992).

Observations and data reduction
===============================

The sample was observed at

-   **Near-infrared** wavelengths, with the *Cerro Tololo Infrared IMager* (CIRIM) at the 1.5 m Ritchey-Chretien Telescope of the Cerro Tololo Inter-American Observatory (CTIO) on October 22- -27, 1998 (Prop0020). CIRIM is equipped with a 256$\times$256-pixel HgCdTe NICMOS3 array (Rockwell Science) with a pixel scale of $1.16 \arcsec$. We observed our sample galaxies through the $K_{\rm{short}}$ filter ($\equiv K_{\rm s}$), characterised by an effective wavelength $\lambda_{\rm eff} = 2.15 \mu$m (Wainscoat & Cowie 1992). We opted for this filter instead of the 