We present VLA 9 mm ( 33 GHz ) observations of the HD 141569 system from semester 16A .
The observations achieve a resolution of 0.25 arcsec ( \sim 28 au ) and a sensitivity of 4.7 ~ { } \mu Jy~ { } beam ^ { -1 } .
We find ( 1 ) a 52 \pm 5 ~ { } \mu Jy point source at the location of HD 141569A that shows potential variability , ( 2 ) the detected flux is contained within the SED-inferred central clearing of the disc meaning the spectral index of the dust disc is steeper than previously inferred , and ( 3 ) the M dwarf companions are also detected and variable .
Previous lower-resolution VLA observations ( semester 14A ) found a higher flux density , interpreted as solely dust emission .
When combined with ALMA observations , the VLA 14A observations suggested the spectral index and grain size distribution of HD 141569 ’ s disc was shallow and an outlier among debris systems .
Using archival ALMA observations of HD 141569 at 0.87 mm and 2.9 mm we find a dust spectral index of \alpha _ { mm } = 1.81 \pm 0.20 .
The VLA 16A flux corresponds to a brightness temperature of \sim 5 \times 10 ^ { 6 } K , suggesting strong non-disc emission is affecting the inferred grain properties .
The VLA 16A flux density of the M2V companion HD 141569B is 149 \pm 9 ~ { } \mu Jy , corresponding to a brightness temperature of \sim 2 \times 10 ^ { 8 } K and suggesting significant stellar variability when compared to the VLA14A observations , which are smaller by a factor of \sim 6 .