NAOC Open IR
Fragmentation of star-forming filaments in the X-shaped nebula of the California molecular cloud
Zhang, Guo-Yin1,2,3; Andre, Ph.2; Men'shchikov, A.2; Wang, Ke4,5
2020-10-06
Source PublicationASTRONOMY & ASTROPHYSICS
ISSN0004-6361
Volume642Pages:14
AbstractContext. Dense molecular filaments are central to the star formation process, but the detailed manner in which they fragment into prestellar cores is not well understood yet. Aims. Here, we investigate the fragmentation properties and dynamical state of several star-forming filaments in the X-shaped nebula region of the California molecular cloud in an effort to shed some light on this issue. Methods. We used multiwavelength far-infrared images from Herschel as well as the getsources and getfilaments extraction methods to identify dense cores and filaments in the region and derive their basic properties. We also used a map of (CO)-C-13(2-1) emission from the Arizona 10m Submillimeter Telescope (SMT) to constrain the dynamical state of the filaments. Results. We identified ten filaments with aspect ratios of AR > 4 and column density contrasts of C > 0.5, as well as 57 dense cores, including two protostellar cores, 20 robust prestellar cores, 11 candidate prestellar cores, and 24 unbound starless cores. All ten filaments have roughly the same deconvolved full width at half maximum (FWHM), with a median value of 0.12 0.03 pc, which is independent of their column densities ranging from <10(21) cm(-2) to >10(22) cm(-2). Two star-forming filaments (# 8 and # 10) stand out since they harbor quasi-periodic chains of dense cores with a typical projected core spacing of similar to 0.15 pc. These two filaments have thermally supercritical line masses and are not static. Filament 8 exhibits a prominent transverse velocity gradient, suggesting that it is accreting gas from the parent cloud gas reservoir at an estimated rate of similar to 40 +/- 10 M-circle dot Myr(-1) pc(-1). Filament 10 includes two embedded protostars with outflows and it is likely at a somewhat later evolutionary stage than filament 8. In both cases, the observed (projected) core spacing is similar to the filament width and significantly shorter than the canonical separation of similar to 4 times the filament width predicted by classical cylinder fragmentation theory. It is unlikely that projection effects can explain this discrepancy. We suggest that the continuous accretion of gas onto the two star-forming filaments, as well as the geometrical bending of the filaments, may account for the observed core spacing. Conclusions. Our findings suggest that the characteristic fragmentation lengthscale of molecular filaments is quite sensitive to external perturbations from the parent cloud, such as the gravitational accretion of ambient material.
Keywordstars: formation ISM: clouds dust extinction ISM: kinematics and dynamics
Funding OrganizationESO-ARO programme ; ESO-ARO programme ; Chinese Government Scholarship ; Chinese Government Scholarship ; French national programs of CNRS/INSU on stellar and ISM physics (PNPS and PCMI) ; French national programs of CNRS/INSU on stellar and ISM physics (PNPS and PCMI) ; National Key Research and Development Program of China ; National Key Research and Development Program of China ; National Science Foundation of China ; National Science Foundation of China ; Kavli Institute for Astronomy and Astrophysics, Peking University ; Kavli Institute for Astronomy and Astrophysics, Peking University ; ESO-ARO programme ; ESO-ARO programme ; Chinese Government Scholarship ; Chinese Government Scholarship ; French national programs of CNRS/INSU on stellar and ISM physics (PNPS and PCMI) ; French national programs of CNRS/INSU on stellar and ISM physics (PNPS and PCMI) ; National Key Research and Development Program of China ; National Key Research and Development Program of China ; National Science Foundation of China ; National Science Foundation of China ; Kavli Institute for Astronomy and Astrophysics, Peking University ; Kavli Institute for Astronomy and Astrophysics, Peking University ; ESO-ARO programme ; ESO-ARO programme ; Chinese Government Scholarship ; Chinese Government Scholarship ; French national programs of CNRS/INSU on stellar and ISM physics (PNPS and PCMI) ; French national programs of CNRS/INSU on stellar and ISM physics (PNPS and PCMI) ; National Key Research and Development Program of China ; National Key Research and Development Program of China ; National Science Foundation of China ; National Science Foundation of China ; Kavli Institute for Astronomy and Astrophysics, Peking University ; Kavli Institute for Astronomy and Astrophysics, Peking University ; ESO-ARO programme ; ESO-ARO programme ; Chinese Government Scholarship ; Chinese Government Scholarship ; French national programs of CNRS/INSU on stellar and ISM physics (PNPS and PCMI) ; French national programs of CNRS/INSU on stellar and ISM physics (PNPS and PCMI) ; National Key Research and Development Program of China ; National Key Research and Development Program of China ; National Science Foundation of China ; National Science Foundation of China ; Kavli Institute for Astronomy and Astrophysics, Peking University ; Kavli Institute for Astronomy and Astrophysics, Peking University
DOI10.1051/0004-6361/202037721
WOS KeywordINTERSTELLAR FILAMENTS ; INITIAL CONDITIONS ; MAGNETIC-FIELDS ; EQUILIBRIUM ; STABILITY ; ROTATION
Language英语
Funding ProjectESO-ARO programme[196.C-0999(A)] ; Chinese Government Scholarship[201804910583] ; French national programs of CNRS/INSU on stellar and ISM physics (PNPS and PCMI) ; National Key Research and Development Program of China[2017YFA0402702] ; National Key Research and Development Program of China[2019YFA0405100] ; National Science Foundation of China[11973013] ; National Science Foundation of China[11721303] ; Kavli Institute for Astronomy and Astrophysics, Peking University[7101502287]
Funding OrganizationESO-ARO programme ; ESO-ARO programme ; Chinese Government Scholarship ; Chinese Government Scholarship ; French national programs of CNRS/INSU on stellar and ISM physics (PNPS and PCMI) ; French national programs of CNRS/INSU on stellar and ISM physics (PNPS and PCMI) ; National Key Research and Development Program of China ; National Key Research and Development Program of China ; National Science Foundation of China ; National Science Foundation of China ; Kavli Institute for Astronomy and Astrophysics, Peking University ; Kavli Institute for Astronomy and Astrophysics, Peking University ; ESO-ARO programme ; ESO-ARO programme ; Chinese Government Scholarship ; Chinese Government Scholarship ; French national programs of CNRS/INSU on stellar and ISM physics (PNPS and PCMI) ; French national programs of CNRS/INSU on stellar and ISM physics (PNPS and PCMI) ; National Key Research and Development Program of China ; National Key Research and Development Program of China ; National Science Foundation of China ; National Science Foundation of China ; Kavli Institute for Astronomy and Astrophysics, Peking University ; Kavli Institute for Astronomy and Astrophysics, Peking University ; ESO-ARO programme ; ESO-ARO programme ; Chinese Government Scholarship ; Chinese Government Scholarship ; French national programs of CNRS/INSU on stellar and ISM physics (PNPS and PCMI) ; French national programs of CNRS/INSU on stellar and ISM physics (PNPS and PCMI) ; National Key Research and Development Program of China ; National Key Research and Development Program of China ; National Science Foundation of China ; National Science Foundation of China ; Kavli Institute for Astronomy and Astrophysics, Peking University ; Kavli Institute for Astronomy and Astrophysics, Peking University ; ESO-ARO programme ; ESO-ARO programme ; Chinese Government Scholarship ; Chinese Government Scholarship ; French national programs of CNRS/INSU on stellar and ISM physics (PNPS and PCMI) ; French national programs of CNRS/INSU on stellar and ISM physics (PNPS and PCMI) ; National Key Research and Development Program of China ; National Key Research and Development Program of China ; National Science Foundation of China ; National Science Foundation of China ; Kavli Institute for Astronomy and Astrophysics, Peking University ; Kavli Institute for Astronomy and Astrophysics, Peking University
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS IDWOS:000578530000002
PublisherEDP SCIENCES S A
Citation statistics
Document Type期刊论文
Identifierhttp://ir.bao.ac.cn/handle/114a11/81941
Collection中国科学院国家天文台
Corresponding AuthorZhang, Guo-Yin
Affiliation1.Chinese Acad Sci, Natl Astron Observ, Beijing 100101, Peoples R China
2.Univ Paris Diderot, Univ Paris Saclay, CNRS, Lab Astrophys AIM,CEA DRF,Sorbonne Paris Cite, F-91191 Gif Sur Yvette, France
3.Univ Chinese Acad Sci, Beijing 100049, Peoples R China
4.Peking Univ, Kavli Inst Astron & Astrophys, 5 Yiheyuan Rd, Beijing 100871, Peoples R China
5.ESO Headquarters, Karl Schwarzschild Str 2, D-85748 Garching, Germany
Recommended Citation
GB/T 7714
Zhang, Guo-Yin,Andre, Ph.,Men'shchikov, A.,et al. Fragmentation of star-forming filaments in the X-shaped nebula of the California molecular cloud[J]. ASTRONOMY & ASTROPHYSICS,2020,642:14.
APA Zhang, Guo-Yin,Andre, Ph.,Men'shchikov, A.,&Wang, Ke.(2020).Fragmentation of star-forming filaments in the X-shaped nebula of the California molecular cloud.ASTRONOMY & ASTROPHYSICS,642,14.
MLA Zhang, Guo-Yin,et al."Fragmentation of star-forming filaments in the X-shaped nebula of the California molecular cloud".ASTRONOMY & ASTROPHYSICS 642(2020):14.
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