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19 April 2024

» arxiv » 1511.9121

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Planck cold clumps in the $lambda$ Orionis complex: I. Discovery of an extremely young Class 0 protostellar object and a proto-brown dwarf candidate in a bright rimmed clump PGCC G192.32-11.88
Tie Liu ; Qizhou Zhang ; Kee-Tae Kim ; Yuefang Wu ; Chang Won Lee ; Jeong-Eun Lee ; Kenichi Tatematsu ; Minho Choi ; Mika Juvela ; Mark Thompson ; Paul F. Goldsmith ; Sheng-yuan Liu ; Hirano Naomi ; Patrick Koch ; Christian Henkel ; Patricio Sanhueza ; JinHua He ; Alana Rivera-Ingraham ; Ke Wang ; Maria R. Cunningham ; Ya-Wen Tang ; Shih-Ping Lai ; Jinghua Yuan ; Di Li ; Gary Fuller ; Miju Kang ; Quang Nguyen Luong ; Hauyu Baobab Liu ; Isabelle Ristorcelli ; Ji Yang ; Ye Xu ; Tomoya Hirota ; Diego Mardones ; Sheng-Li Qin ; Huei-Ru Chen ; Woojin Kwon ; FanYi Meng ; Huawei Zhang ; Mi-Ryang Kim ; Hee-Weon Yi ;
Date:	25 Nov 2015
Abstract:	We are performing a series of observations with ground-based telescopes toward Planck Galactic cold clumps (PGCCs) in the $lambda$ Orionis complex in order to systematically investigate the effects of stellar feedback. In the particular case of PGCC G192.32-11.88, we discovered an extremely young Class 0 protostellar object (G192N) and a proto-brown dwarf candidate (G192S). G192N and G192S are located in a gravitationally bound bright-rimmed clump. The velocity and temperature gradients seen in line emission of CO isotopologues indicate that PGCC G192.32-11.88 is externally heated and compressed. G192N probably has the lowest bolometric luminosity ($sim0.8$ L$_{sun}$) and accretion rate (6.3$ imes10^{-7}$ M$_{sun}$~yr$^{-1}$) when compared with other young Class 0 sources (e.g. PACS Bright Red sources (PBRs)) in the Orion complex. It has slightly larger internal luminosity ($0.21pm0.01$ L$_{sun}$) and outflow velocity ($sim$14 km~s$^{-1}$) than the predictions of first hydrostatic cores (FHSCs). G192N might be among the youngest Class 0 sources, which are slightly more evolved than a FHSC. Considering its low internal luminosity ($0.08pm0.01$ L$_{odot}$) and accretion rate (2.8$ imes10^{-8}$ M$_{sun}$~yr$^{-1}$), G192S is an ideal proto-brown dwarf candidate. The star formation efficiency ($sim$0.3\%-0.4\%) and core formation efficiency ($sim$1\%) in PGCC G192.32-11.88 are significantly smaller than in other giant molecular clouds or filaments, indicating that the star formation therein is greatly suppressed due to stellar feedback.
Source:	arXiv, 1511.9121
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