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• W2316246155 endingPage "114" @default.
• W2316246155 startingPage "114" @default.
• W2316246155 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 $sim2.5times10^3,M_odot$, and the mass of SMM1 is $sim5.5times10^2,M_odot$ 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." @default.
• W2316246155 created "2016-06-24" @default.
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• W2316246155 date "2016-05-13" @default.
• W2316246155 modified "2023-10-16" @default.
• W2316246155 title "COEVAL INTERMEDIATE-MASS STAR FORMATION IN N4W" @default.
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• W2316246155 doi "https://doi.org/10.3847/0004-637x/822/2/114" @default.
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