# Dynamical timescale of precollapse evolution inferred from chemical distribution in the Taurus Molecular Cloud-1 (TMC-1) filament

## TL;DR

This study investigates the chemical distribution and dynamical evolution of the TMC-1 filament in Taurus, revealing how different chemical depletion patterns relate to the region's collapse timescales and star formation activity.

## Contribution

It provides new insights into the relationship between chemical distributions and dynamical timescales in a star-forming filament through combined observations and chemical modeling.

## Key findings

- CO depletion is more significant in the ammonia peak than in the cyanopolyyne peak.
- N2H+ shows little depletion in either peak.
- Chemical distribution differences are explained by varying dynamical timescales.

## Abstract

We present observations and analysis of the low-mass star-forming region, Taurus Molecular Cloud-1 (TMC-1). CS ($J$=2-1)/N$_2$H$^+$ ($J$=1-0) and C$^{17}$O ($J$=2-1)/C$^{18}$O ($J$=2-1) were observed with FCRAO (Five College Radio Astronomy Observatory) and SRAO (Seoul Radio Astronomy Observatory), respectively. In addition, Spitzer infrared data and 1.2 mm continuum data observed with MAMBO (Max-Planck Millimetre Bolometer) are used. We also perform chemical modeling to investigate the relative molecular distributions of the TMC-1 filament. Based on Spitzer observations, there is no young stellar object along the TMC-1 filament, while five Class II and one Class I young stellar objects are identified outside the filament. The comparison between column densities calculated from dust continuum and C$^{17}$O 2-1 line emission shows that CO is depleted much more significantly in the ammonia peak than in the cyanopolyyne peak, while the column densities calculated from the dust continuum are similar at the two peaks. N$_2$H$^+$ is not depleted much in either peak. According to our chemical calculation, the differential chemical distribution in the two peaks can be explained by different timescales required to reach the same density, i.e., by different dynamical processes.