# An Estimation of the Star Formation Rate in the Perseus Complex

## TL;DR

This paper estimates the star formation rate in the Perseus complex by analyzing cores and YSOs, finding most starless cores are unstable and likely to form new stars, with a proposed one-to-one relation between cores and protostars.

## Contribution

It introduces a detailed analysis linking starless cores and YSOs, proposing a constant star formation rate based on their observed relation.

## Key findings

- Most starless cores in Perseus are unstable and likely to collapse.
- The estimated star formation rate is approximately 150 solar masses per million years.
- A one-to-one relation between starless cores and protostars suggests a steady star formation process.

## Abstract

We present the results of our investigation of the star-forming potential in the Perseus star-forming complex. We build on previous starless core, protostellar core, and young stellar object (YSO) catalogs from Spitzer, Herschel, and SCUBA observations in the literature. We place the cores and YSOs within seven star-forming clumps based on column densities greater than 5x10^21 cm^-2. We calculate the mean density and free-fall time for 69 starless cores as 5.55x10^-19 gcm^-3 and 0.1 Myr,respectively, and we estimate the star formation rate for the near future as 150 Msun Myr^-1. According to Bonnor Ebert stability analysis, we find that majority of starless cores in Perseus are unstable. Broadly, these cores can collapse to form the next generation of stars. We found a relation between starless cores and YSOs, where the numbers of young protostars (Class 0 + Class I) are similar to the numbers of starless cores. This similarity, which shows a one-to-one relation, suggests that these starless cores may form the next generation of stars with approximately the same formation rate as the current generation, as identified by the Class 0 and Class I protostars. It follows that if such a relation between starless cores and any YSO stage exists, the SFR values of these two populations must be nearly constant. In brief, we propose that this one-to-one relation is an important factor in better understanding the star formation process within a cloud.