<div>Very Low Luminosity Objects (VeLLOs) are deeply embedded and extremely faint objects. In order to pinpoint the origins of chemical complexity in interstellar space it is crucial to learn about chemical processes that occur in those types of sources. The nature and future evolution of VeLLOs is currently under debate, as only a handful of sources have been studied in detail. Whether they are young Class 0 sources (e.g., Dunham et al. 2006), extremely low-mass protostars or proto-brown dwarf candidates (e.g., Palau et al. 2014), or objects in the quiescent phase of an episodic accretion burst (Dunham et al. 2010) is still an open question. <br></div><div>I will present Atacama Pathfinder Experiment (APEX) observations of the isolated VeLLO in the DC3272+18 dark cloud that has recently undergone an accretion outburst, as inferred by the current position of its CO snowline (Hsieh et al. 2018). I will show molecular tracers of the kinematic and dynamic structures of the VeLLO, and discuss how the gas-phase detections of molecules such as methanol (CH3OH), formaldehyde (H2CO), and nitric oxide (NO) can be attributed to its past outburst. <br></div><div>Studying the chemical evolution across multiple stages of star-formation is vital to understand the emergence and inheritance of chemical complexity in space. Characterizing the chemical inventories of VeLLOs is a crucial stepping-stone for linking pre- and protostellar stages. Thus, I will conclude by comparing the derived line intensity and molecular abundance ratios from the VeLLO in DC3272+18 with molecular clouds and low-mass protostars. <br></div><div>References:
Dunham et al. 2006, ApJ, 651, 945
Dunham et al. 2010, ApJ, 721,995
Hsieh et al. 2018, ApJ, 854, 15
Palau et al. 2014, MNRAS, 444, 833
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