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Our aim was to directly detect the thermal emission of the putative exoringsystem responsible for the complex deep transits observed in the light curvefor the young Sco-Cen star 1SWASP J140747.93-394542.6 (V1400 Cen, hereafterJ1407), confirming it as the occulter seen in May 2007, and to determine itsorbital parameters with respect to the star. We used the Atacama LargeMillimeter/submillimeter Array (ALMA) to observe the field centred on J1407 inthe 340 GHz (Band 7) continuum in order to determine the flux and astrometriclocation of the ring system relative to the star. We used the VLT/NACO camerato observe the J1407 system in March 2019 and to search for the centralplanetary mass object at thermal infrared wavelengths. We detect no pointsource at the expected location of J1407, and derive an upper limit $3\sigma$level of $57.6~\mu\rm{Jy}$. There is a point source detected at an angularseparation consistent with the expected location for a free-floating ringsystem that occulted J1407 in May 2007, with a flux of $89~\mu\rm{Jy}$consistent with optically thin dust surrounding a massive substellar companion.At 3.8 microns with the NACO camera, we detect the star J1407 but no otheradditional point sources within 1.3 arcseconds of the star, with a lower boundon the sensitivity of $6M_{Jup}$ at the location of the ALMA source, and downto $4M_{Jup}$ in the sky background limit. The ALMA upper limit at the locationof J1407 implies that a hypothesised bound ring system is composed of dustsmaller than $1\rm{~mm}$ in size, implying a young ring structure. The detectedALMA source has multiple interpretations, including: (i) it is an unboundsubstellar object surrounded by warm dust in Sco-Cen with an upper mass limitof $6M_{Jup}$, or (ii) it is a background galaxy.

ALMA and NACO observations towards the young exoring transit system J1407 (V1400 Cen)