Coeval intermediate-mass star formation in N4W

TL;DR

This study investigates the properties and star formation processes in the N4W region, revealing coeval intermediate-mass star formation with evidence of outflows, temperature variations, and potential for massive star formation.

Contribution

It provides detailed multi-wavelength observations and analysis of N4W, demonstrating nearly coeval formation of intermediate-mass stars and identifying a gravitationally bound submillimeter source capable of forming massive stars.

Findings

Identification of multiple YSOs with outflows in N4W

Presence of two dust temperature distributions

Potential for massive star formation in SMM1

Abstract

Protostars are mostly found in star-forming regions, where the natal molecular gas still remains. In about 5' west of the molecular bubble N4, N4W is identified as a star-forming clump hosting three Class II (IRS\,1\,--\,3), and one Class I (IRS\,4) young stellar objects (YSOs), as well as a submillimeter source SMM1. The near-IR polarization imaging data of N4W reveal two infrared reflection nebulae close to each other, which are in favor of the outflows of IRS\,1 and IRS\,2. The bipolar mid-IR emission centered on IRS\,4 and the arc-like molecular gas shell are lying on the same axis, indicating a bipolar molecular outflow from IRS\,4. There are two dust temperature distributions in N4W. The warmer one is widely distributed and has a temperature $T_\mathrm{d}\gtrsim28\,\mathrm{K}$, with the colder one from the embedded compact submillimeter source SMM1. N4W's mass is estimated to be $\sim2.5\times10^3\,M_\odot$, and the mass of SMM1 is $\sim5.5\times10^2\,M_\odot$ at $T_\mathrm{d}=15\,\mathrm{K}$, calculated from the CO\,$1-0$ emission and $870\,\mu$m dust continuum emission, respectively. Based on the estimates of bolometric luminosity of IRS\,1\,--\,4, these four sources are intermediate-mass YSOs at least. SMM1 is gravitationally bound, and is capable of forming intermediate-mass stars or even possibly massive stars. The co-existence of the IR bright YSOs and the submillimeter source represents potential sequential star formation processes separated by $\sim0.5$\,Myr in N4W. This small age spread implies that the intermediate-mass star formation processes happening in N4W are almost coeval.