منابع مشابه
Clustered Star Formation in W 75
We present 2 ′′ to 7 ′′ resolution 3 mm continuum and CO(J=1−0) line emission and near infrared K s , H 2 , and [FeII] images toward the massive star forming region W75 N. The CO emission uncovers a complex morphology of multiple, overlapping outflows. A total flow mass of > 255 M ⊙ extends 3 pc from end-to-end and is being driven by at least four late to early-B protostars. More than 10% of th...
متن کاملClustered Massive Star Formation in Molecular Clouds
I review some important questions in the field of massive star formation: What are the initial conditions for proto star clusters and how do they arise? What are the initial conditions for individual massive star formation within star clusters? How do massive protostars accumulate their mass? I compare the Turbulent Core Model (McKee & Tan 2003) to several nearby regions, including Orion KL. He...
متن کاملStatistical Analysis of Water Masers in Star-forming Regions: Cepheus a and W75 N
We have done a statistical analysis of Very Long Baseline Array (VLBA) data of water masers in the star-forming regions (SFRs) Cepheus A and W75 N, using correlation functions to study the spatial clustering and Doppler-velocity distribution of these masers. Two-point spatial correlation functions show a characteristic scale size for clusters of water maser spots .1 AU, similar to the values fo...
متن کاملBeyond the nuclear starburst? Clustered star formation in major mergers
Recent simulation work has successfully captured the formation of the star clusters that have been observed in merging galaxies. These studies, however, tend to focus on studying extreme starbursts, such as the Antennae galaxies. We aim to establish whether there is something special occurring in these extreme systems or whether the mechanism for cluster formation is present in all mergers to a...
متن کاملThickening of galactic disks through clustered star formation
The building blocks of galaxies are star clusters. These form with low-star formation efficiencies and, consequently, loose a large part of their stars that expand outwards once the residual gas is expelled by the action of the massive stars. Massive star clusters may thus add kinematically hot components to galactic field populations. This kinematical imprint on the stellar distribution functi...
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ژورنال
عنوان ژورنال: The Astrophysical Journal
سال: 2003
ISSN: 0004-637X,1538-4357
DOI: 10.1086/345743