Qiu Zhang

Nature of two massive protostellar candidates: IRAS 21307+5049 and IRAS 22172+5549

We present observations of continuum and molecular lines towards the protostar candidates IRAS 21307+5049 and IRAS 22172+5549. Single-dish maps in the 12 COu2000(2–1), C 18 Ou2000(2–1), H 13 CO + u2000(1–0) lines and 850 μ m continuum are compared with interferometric maps in the 12 COu2000(1–0) line and 3xa0mm continuum, and with mid- and near-infrared images. Also, single-pointing spectra of the CH 3 C 2 Hu2000(6–5), (8–7) and (13–12) lines observed towards IRAS 21307+5049, and H 2 andxa0[FeII]xa0line emission observed towards IRAS 22172+5549, are presented. A plausible interpretation of our data based on the continuum maps and spectral energy distributions is that two components are present: a compact molecular core, responsible for the continuum emission at wavelengths longer than ~

Little Massive Substructure in CMZ Molecular Clouds

25;mu

The gentle CMF of high-mass star-forming regions

m, and a cluster of stars located close to the center of the core, but not spatially coincident with it, responsible for the emission at shorter wavelengths. The core is approximately located at the center of the associated molecular outflow, detected for both sources in the 12 COu2000(1–0) and (2–1) lines. The cores have masses of ~

Studying Infall in Cluster Forming Scales with the Submillimeter Array

50;M_{odot}

Spitzer IRAC and MIPS Observations toward High-mass Star Forming Regions

, and luminosities of ~

SMA Imaging of Massive Star Formation in NGC6334I and I(N)

10^{3};L_{odot}

Jet-like Molecular Outflows in Massive Young Stars

. The outflows parameters are consistent with those typically found in high-mass young stellar objects. u2029Our results support the hypothesis that in these sources the luminosity is dominated by accretion rather than by nuclear burning. We conclude that the sources embedded inside the cores are likely protostars with mass ~

IRAS 18317-0757: A Cluster of Massive Stars and Protostars

5{-}8;M_{odot}

High-Mass Protostars

.