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        Planck Cold Clumps in the λ Orionis Complex. I : Discovery of an Extremely Young Class 0 Protostellar Object and a Proto-brown Dwarf Candidate in the Bright-rimmed Clump PGCC G192.32-11.88

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        Author
        Liu, T.
        Zhang, Q.
        Kim, K.-T.
        Wu, Y.
        Lee, C.W.
        Lee, J.-E.
        Tatematsu, K.
        Choi, M.
        Juvela, M.
        Thompson, M.A.
        Goldsmith, P.F.
        Liu, S.Y.
        Naomi, H.
        Koch, P.
        Henkel, C.
        Sanhueza, P.
        He, J.
        Rivera-Ingraham, A.
        Wang, K.
        Cunningham, M.R.
        Tang, Y.-W.
        Lai, S.-P.
        Yuan, J.
        Li, D.
        Fuller, G.
        Kang, M.
        Nguyen Luong, Q.
        Liu, H.B.
        Ristorcelli, I.
        Yang, J.
        Xu, Y.
        Hirota, T.
        Mardones, D.
        Qin, S.-L.
        Chen, H.-R.
        Kwon, W.
        Meng, F.
        Zhang, H.
        Kim, M.-R.
        Yi, H.-W.
        Attention
        2299/16805
        Abstract
        We are performing a series of observations with ground-based telescopes toward Planck Galactic cold clumps (PGCCs) in the λ 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 (˜0.8 {L}⊙ ) and accretion rate (6.3 × 10-7 {M}⊙ yr-1) when compared with other young Class 0 sources (e.g., PACS Bright Red Sources) in the Orion complex. It has slightly larger internal luminosity (0.21 ± 0.01 {L}⊙ ) and outflow velocity (˜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 an FHSC. Considering its low internal luminosity (0.08 ± 0.01 {L}⊙ ) and accretion rate (2.8 × 10-8 {M}⊙ yr-1), G192S is an ideal proto-brown dwarf candidate. The star formation efficiency (˜0.3%-0.4%) and core formation efficiency (˜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 owing to stellar feedback.
        Publication date
        2016-01-14
        Published in
        Astrophysical Journal, Supplement Series
        Published version
        https://doi.org/10.3847/0067-0049/222/1/7
        Other links
        http://hdl.handle.net/2299/16805
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