2019MNRAS.487.2853Y

The first stable object to develop in the low-mass star formation process has long been predicted to be the first hydrostatic core (FHSC). Despite much effort, it has still yet to be definitively observed in nature. More specific observational signatures are required to enable observers to distinguish the FHSC from young, faint, but more evolved protostars. Here, we present synthetic spectral line observations for CO, SO, CS, and HCO⁺ that were calculated from radiation (magneto)hydrodynamical models, chemical modelling, and Monte Carlo radiative transfer. HCO⁺ (1 - 0) and SO (8₇ - 7₆) spectra of the FHSC show variations for observations at a low inclination which may allow a candidate FHSC to be distinguished from a more evolved object. We find that the FHSC outflow is unlikely to be detectable with ALMA (Atacama Large Millimeter/Submillimeter Array), which would discount the observed sources with slow outflows that are currently identified as candidate FHSCs. We compare the results of simulated ALMA observations with observed candidate FHSCs and recommend Oph A SM1N and N6-mm as the most promising candidates to follow up.