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It is known that massive stars form as result of the fragmentation ofmolecular clumps. However, what is not clear is whether this fragmentationgives rise to cores massive enough to form directly high-mass stars, or leadsto cores of low and intermediate mass that generate massive stars acquiringmaterial from their environment. Detailed studies towards clumps at earlystages of star formation are needed to collect observational evidence that shedlight on this issue. The infrared-quiet massive clump AGAL G035.1330-00.7450,located at a distance of 2.1 kpc, is a promising object to study both thefragmentation and the star formation activity at early stages. Using millimeterobservations of continuum and molecular lines obtained from the Atacama LargeMillimeter Array database at Bands 6 and 7, we study the substructure of thissource. The angular resolution of the data at Band 7 is about 0\farcs7, whichallow us to resolve structures of about 0.007 pc ($\sim$1500 au). We found thatthe clump harbours four dust cores (C1-C4) with masses below 3 M$_{\odot}$.Cores C3 and C4 exhibit well collimated, young, and low-mass molecularoutflows. C1 and C2 present CH$_3$CN J=13--12 emission, from which we deriverotational temperatures of about 180 and 100 K, and masses of about 1.4 and 0.9M$_{\odot}$, respectively. The moment 1 map of the CH$_3$CN emission suggeststhe presence of a rotating disk towards C1, which is confirmed by the CH$_3$OHand CH$_3$OCHO (20-19) emissions. On the other hand, CN N=2-1 emission shows aclumpy and filamentary structure that seems to connect all the cores. Thesefilaments might be tracing the remnant gas of the fragmentation processestaking place within the clump, or gas that is being transported towards thecores, which would imply a competitive accretion scenario.

Unveiling the substructure of the massive clump AGAL G035.1330$-$00.7450