HC$_3$N, H$^{13}$CN, and HN$^{13}$C in molecular cores evolving towards star-forming regions

TL;DR

This study analyzes molecular cores in early star formation stages using ALMA data, focusing on specific molecules to understand initial interstellar conditions and their relation to temperature.

Contribution

It provides new chemical and physical insights into early star-forming cores by analyzing molecular abundances and their correlation with temperature.

Findings

H$^{13}$CN and HN$^{13}$C abundances increase with temperature

HC$_3$N shows no correlation with temperature

Spectral analysis of 37 sources reveals molecular abundance patterns

Abstract

As a work in progress, results from a chemical and physical analysis of molecular cores in early evolutionary stages concerning star formation are presented. Using archival data from the Atacama Large Millimeter Array (ALMA), a sample of 37 sources was investigated, from which spectra in the frequency range 330--350 GHz were extracted towards the central positions of the molecular cores. Transitions of HC$_3$N, H$^{13}$CN, and HN$^{13}$C were analysed using Gaussian fits, obtaining peak intensities, fluxes, and line widths. The column densities of each molecule and their abundances were estimated. The behaviour of these abundances with the temperature of the region was studied, observing positive correlations for H$^{13}$CN and HN$^{13}$C, and none for HC$_3$N. This study contributes to the characterisation of the initial conditions of the interstellar medium in early phases of stellar evolution.