# Synthetic molecular line observations of the first hydrostatic core from chemical calculations

## TL;DR

This study uses synthetic spectral line observations from advanced models to identify potential observational signatures of the elusive first hydrostatic core in star formation, aiding its detection.

## Contribution

It provides the first detailed synthetic spectral analysis of the FHSC using combined chemical and radiative transfer models, suggesting specific observational signatures.

## Key findings

- HCO+ and SO spectra show potential signatures at low inclination.
- Most FHSC outflows are undetectable with ALMA, explaining current observational challenges.
- Oph A SM1N and N6-mm are promising candidates for future observations.

## Abstract

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 $(8_7 - 7_6)$ 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, 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.