1 Introduction

The globule DC 303.8-14.2 (Hartley et al. 1986) is located in the eastern part of the Chamaeleon II dark cloud complex. It harbours the IRAS point source IRAS 13036-7644, which possesses a spectral energy distribution (SED) typical for a young stellar object (YSO); the flux densities at 12, 25, 60 and 100 $\mu$m are 0.10, 1.08, 6.28 and 22.01 Jy, respectively (Prusti et al. 1992). Its coordinates are $\alpha(1950)=13^{\rm h} 3^{\rm m} 41.4^{\rm s}$, $\delta(1950)=-76\hbox{$^\circ$ }44\hbox{$^\prime$ }3\hbox{$^{\prime\prime}$ }$, and the positional error ellipse has semi minor and major axes of 6$\hbox {$^{\prime \prime }$ }$ and 20$\hbox {$^{\prime \prime }$ }$.

In their continuum survey at 1.3 mm Henning et al. (1993) measured a flux density of $223 \pm 49$ mJy for this object. This emission is most probably thermal emission from cold circumstellar dust grains.

Lehtinen (1997) has observed DC 303.8-14.2 at millimeter molecular lines, and found that the high density tracers CS(J=2-1), CS(J=3-2) and H₂CO(2₁₂-1₁₁) show asymmetrical douple-peaked profiles that are typical for a collapsing cloud. IRAS 13036-7644 is located at the center of a bipolar molecular outflow; thus it is probably the driving source of this outflow (Lehtinen 1997), although it is possible that another, even younger source could be driving the outflow. In addition, there seems to be another red-shifted outflow component at ( $\Delta \alpha, \Delta \delta) \approx (-4\hbox{$^\prime$ }, -2\hbox{$^\prime$ }$), and possibly a blue-shifted outflow component located to the west from it (see Fig. 1).

Chen et al. (1997) have calculated bolometric luminosities and temperatures (as defined in Myers & Ladd 1993) for YSOs in nearby molecular clouds. They find values of 0.47 $L_{\odot}$ and 63 K for IRAS 13036-7644. In a bolometric luminosity-temperature diagram of Chen et al. (1995) IRAS 13036-7644 is located near the division line between Class 0 and Class I sources. However, in the absence of flux measurements between 100 $\mu$m and 1.3 mm it is not possible to deduce reliably the class of the IRAS source.

It is known that even very low luminosity sources associated with bipolar outflows produce radio continuum emission. In the context of Bok globules, Yun et al. (1996) have searched for radio continuum emission from globules using the VLA at 3.6 cm, and found that most of the globules that have a radio continuum source within their optical extent, have been previously found to have an associated molecular outflow. This relationship between continuum radiation and outflows led Yun et al. (1996) to suggest that the continuum radiation is coming from circumstellar gas which is shock-ionized by the stellar wind from the YSO. This stellar wind is also the power source of the molecular outflow.

The youngest stellar objects known so far (possibly true protostars, so called Class 0 objects) are so deeply embedded in their parent cloud that they are detectable only at mid-infrared and at longer wavelengths. Sometimes these objects can be detected only due to the associated molecular outflow, and by means of their cm-wavelength continuum radiation. Most of the objects that have been classified as Class 0 objects have also been detected in centimeter wavelength continuum radiation (Yun et al. 1996).

The main motivation of this study was to detect cm-wavelength continuum radiation from the IRAS 13036-7644. Radio flux measurements would complement the existing SED, and permit the determination of a more accurate luminosity. The spectral index, $\alpha$ (defined to be $S_{\nu} \propto \nu^{\alpha}$), of the emission between 3 and 6 cm can be used to distinguish between the various emission mechanisms. Our observations could also reveal new YSOs that are so heavily embebbed that they are not detected by IRAS, i.e. possible Class 0 objects.