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研究生： 穆美蓉
Nadia M. Murillo
論文名稱： 抽絲剝繭：非同時代三合一原恆星系統VLA1623之觀測與分析
Disentangling the Entangled: Observations and analysis of the triple non-coeval protostellar system VLA1623
指導教授： 賴詩萍
Lai, Shih-Ping
口試委員: 李景輝
Lee, Chin-Fei
平野尚美
Naomi Hirano
學位類別： 碩士
Master
系所名稱： 理學院 - 天文研究所
Institute of Astronomy
論文出版年： 2012
畢業學年度： 100
語文別： 英文
論文頁數： 56
中文關鍵詞： 原恆星 、天文 、恆星形成 、無線電天文學 、觀測
外文關鍵詞： Multiple Protostellar Systems, Radio Astronomy, Atacama Large Millimeter/submillimeter Array ALMA, Submillimeter Array SMA
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    • Multiple Protostellar Systems (MPSs) are common at every evolutionary
    stage, and yet their formation and evolution are still little understood. Models and
    simulations predict that MPSs most likely form through fragmentation, but the ques-
    tions of when and how are still left widely open. Continuum surveys of MPSs have
    been performed at every evolutionary stage, but the results can only address the mul-
    tiplicity distribution. To fully understand and constrain the formation and evolution
    mechanisms of MPSs, the multiplicity, coevality, outflow and circumstellar environ-
    ment must be addressed. MPSs present many chanllenges, as they can be deeply en-
    tangled through dynamical evolution and internal interaction. Disentangling MPSs,
    however, can prove to be rewarding, revealing not only insight into the system but
    providing a true star formation laboratory. To achieve this goal, a thorough look
    into a MPS is needed. In this work, we present one such thorough investigation into
    the much debated protostellar system VLA1623, located in ρ Ophiuchi (L1688) at
    a distance of 120pc. Here millimeter, submillimeter and infrared observations and
    archival data along with data from literature are used to present an almost complete
    picture VLA1623. The results and analysis presented in this work provide surprising
    and interesting insight into this system, revealing VLA1623 to be a triple non-coeval
    protostellar system, with each source driving its own outflow and two sources driving
    jets as well as unevenly distributed circumstellar material. Finally, one component,
    VLA1623B, is found to be an extremely young protostellar source with characteristics
    between a starless core and a Class 0 object.

    Abstract ii Acknowledgements iii List of Figures viii List of Tables ix 1 Introduction 1 1.1 Background . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 1 1.2 VLA1623 . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 4 2 Data . . . . . . . . . . . . . . . . . . . . . . . . . 6 2.1 Observations . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 6 2.1.1 SMA . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 6 2.1.2 ALMA . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 8 2.2 Archival Data . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 8 2.3 Collaborations and other data 9 3 Results . . . . . . . . . . . . . . . . . . . . . . . . 10 3.1 Continuum . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 10 3.2 Outflows . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 13 3.3 Circumstellar environment . . . . . . . . . . . . . . . . . . . . . . . . . . . . 15 3.3.1 SO (9-8) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 15 3.3.2 C17 O (3-2) & C18 O (2-1) . . . . . . . . . . . . . . . . . . . . . . . . 15 3.4 ALMA Observations . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 19 3.4.1 12 CO (2-1) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 19 3.4.2 C18 O (2-1) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 19 3.4.3 DCO+ (3-2) . . . . . . . . 19 4 Analysis 23 4.1 Spectral Energy Distribution . . . . . . . . . . . . . . . . . . . . . . . . . . 23 4.2 Physical Parameters . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 24 4.2.1 Bolometric and Submillimeter Luminosities (Lbol & Lsubmm ) . . . . . 26 4.2.2 Envelope Mass (Menv ) . . . . . . . . . . . . . . . . . . . . . 26 4.2.3 Column and Number Densitites (NH2 & nH2 ) . . . . . . . . 27 4.2.4 On undersampled SEDs, luminosities and Error in derived physical parameters . . . . . . . . . . . . . . . . . . . . . . . . . . . 27 4.3 Outflows and Jets . . . . . . . . . . . . . . . . . . . . . . . . . . . 28 4.3.1 12 CO outflows . . . . . . . . . . . . . . . . . . . . . . . . . 28 4.3.2 Jets in H2 and IRAC 2 . . . . . . . . . . . . . . . . . . . . 29 4.4 Circumstellar Envelope . . . . . . . . . . . . . . . . . . . . . . . . . 35 4.4.1 SO (9-8) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 35 4.4.2 C17 O (3-2) & C18 O (2-1) . . . . . . . . . . . . . . . . . . . 35 4.4.3 DCO+ (3-2) . . . . . . . . . . . . . . . . . . . . . . . . . . 38 5 Discussion 42 5.1 VLA1623W . . . . . . . . . . . . 42 5.2 VLA1623A . . . . . . . . . . . . 44 5.3 VLA1623B . . . . . . . . . . . . 45 5.4 A model for VLA1623’s outflows . . . . . . . . . . . . 46 5.5 Formation Scenario . . . . . . . . 46 6 Conclusions 49 Bibliography 50 A Equations and Methods to derive Physical Parameters 55 A.1 Total Mass Mtot . . . . . . . . . . . . . . . . . . . . . . . . 55 A.2 Density . . . . . . . . . . . . . . . . . . . . . . . . . . . . 55 A.2.1 Column Density NH2 . . . . . . . . . . . . . . . . . 55 A.2.2 Number Density nH2 . . . . . . . . . . . . . . . . . 56 A.3 Luminosity . . . . . . . . . . . . . . . . . . . . . . . . . . 56 A.3.1 Bolometric and Submillimeter Luminosity . . . . . . . . . . 56

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