The sequence of low and high mass star formation in the young stellar cluster IRAS 19343+2026

TL;DR

This study investigates the stellar content and formation sequence in the young cluster IRAS 19343+2026, revealing low-mass stars form before massive stars, with detailed photometric and spectroscopic analysis supporting this formation scenario.

Contribution

It provides the first detailed characterization of the stellar population and formation sequence in IRAS 19343+2026 using multi-wavelength data and spectroscopy.

Findings

The cluster contains a massive protostar of 7.6 Msol and early B-type stars.

Low-mass stars are older (1-3 Myr) than the massive protostar (~10^5 yr).

The IMF slope is shallower than Salpeter's prediction.

Abstract

BVRIJHK photometry, Spitzer-GLIMPSE photometry and HK band spectroscopy were used to study the stellar content of IRAS 19343+2026, a (proto)star/cluster candidate, located close to the Galactic plane. The data suggest that IRAS 19343+2026 is a rich cluster associated with a massive protostar of 7.6 Msol with an age of ~ 10^5 yr. Three point sources in the vicinity of the far-infrared (FIR) peak are also found to be early B type stars. The remaining (predominantly low mass) members of the cluster are best represented by a 1 - 3 Myr pre-main-sequence (PMS) population. HK band spectra of two bright and five faint point sources in the cluster confirm that the results obtained from the photometry are good representations of their young stellar object (YSO) nature. Thus, IRAS 19343+2026 is a young cluster with at least four early B-type stars classified as young (10^4 - 10^5 yr), that are surrounded by a somewhat older (1 - 3 Myr) population of low mass YSOs. Together, these results argue for a scenario in which low mass stars form prior to massive stars in a cluster forming environment. We compute the Initial Mass Function (IMF) for this cluster using the K-band luminosity function; the slope of the IMF is shallower than predicted by the Salpeter's mass function. The cluster mass, Mtot, is estimated to be in the range ~ 307 Msol (from the data completeness limit) - 585 Msol (extrapolated down to the brown dwarf limit, assuming a certain IMF).