We present sensitive 1–3 GHz ATCA radio continuum observations of the hitherto unresolved star forming region known as either IRAS 14482–5857 or PMN 1452–5910 .
At radio continuum frequencies , this source is characterised by a “ filled-bubble ” structure reminiscent of a classical H ii region , dominated by three point sources , and surrounded by low-surface-brightness emission out to the \sim 3 ^ { \prime } \times 4 ^ { \prime } source extent observed at other frequencies in the literature .
The infrared emission corresponds well to the radio emission , with polycyclic aromatic hydrocarbon emission surrounding regions of hot dust towards the radio bubbles .
A bright 4.5 \mu m point source is seen towards the centre of the radio source , suggesting a young stellar object .
There is also a linear , outflow-like structure radiating brightly at 8 and 24 \mu m towards the brightest peak of the radio continuum .
In order to estimate the distance to this source , we have used Mopra Southern Galactic Plane CO Survey ^ { 12 } CO ( 1–0 ) and ^ { 13 } CO ( 1–0 ) molecular line emission data .
Integrated-intensity , velocity at peak intensity and line-fitting of the spectra all point towards the peak centred at V _ { LSR } = -1.1 km/s being connected to this cloud .
This infers a distance to this cloud of \sim 12.7 kpc .
Assuming this distance , we estimate a column density and mass towards IRAS 14482–5857 of \sim 1.5 \times 10 ^ { 21 } cm ^ { -2 } and 2 \times 10 ^ { 4 } M _ { \odot } , implying that this source is a site of massive star formation .
Reinforcing this conclusion , our broadband spectral fitting infers dust temperatures of 19 and 110 K , emission measures for the sub-pc radio point-source of EM \sim 10 ^ { 6 - 7 } pc cm ^ { -6 } , electron densities of n _ { e } \sim 10 ^ { 3 } cm ^ { -3 } and photon ionisation rates of N _ { Ly } \sim 10 ^ { 46 - 48 } s ^ { -1 } .
The evidence strongly suggests that IRAS 14482–5857 is a distant – hence intense – site of massive star-formation .