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We present VLA 9 mm (33 GHz) observations of the HD 141569 system fromsemester 16A. The observations achieve a resolution of 0.25 arcsec ($\sim28$au) and a sensitivity of $4.7~\mu \rm Jy~beam^{-1}$. We find (1) a $52\pm5~\mu$Jy point source at the location of HD 141569A that shows potentialvariability, (2) the detected flux is contained within the SED-inferred centralclearing of the disc meaning the spectral index of the dust disc is steeperthan previously inferred, and (3) the M dwarf companions are also detected andvariable. Previous lower-resolution VLA observations (semester 14A) found ahigher flux density, interpreted as solely dust emission. When combined withALMA observations, the VLA 14A observations suggested the spectral index andgrain size distribution of HD 141569's disc was shallow and an outlier amongdebris systems. Using archival ALMA observations of HD 141569 at 0.87 mm and2.9 mm we find a dust spectral index of $\alpha_{\rm mm} = 1.81\pm 0.20$. TheVLA 16A flux corresponds to a brightness temperature of $\sim5\times10^{6}$ K,suggesting strong non-disc emission is affecting the inferred grain properties.The VLA 16A flux density of the M2V companion HD 141569B is $149\pm9~\mu$Jy,corresponding to a brightness temperature of $\sim2\times10^{8}$ K andsuggesting significant stellar variability when compared to the VLA14Aobservations, which are smaller by a factor of $\sim6$.

ALMA and VLA Observations of the HD 141569 System