Fragmentation, rotation, and outflows in the high-mass star-forming region IRAS 23033+5951 A case study of the IRAM NOEMA large program CORE

被引：18

作者：

Bosco, F. ^{[1
,18
]}

Beuther, H. ^{[1
]}

Ahmadi, A. ^{[1
,18
]}

Mottram, J. C. ^{[1
]}

Kuiper, R. ^{[1
,2
]}

Linz, H. ^{[1
]}

Maud, L. ^{[3
]}

Winters, J. M. ^{[4
]}

Henning, T. ^{[1
]}

Feng, S. ^{[5
,19
]}

Peters, T. ^{[6
]}

Semenov, D. ^{[1
,7
]}

Klaassen, P. D. ^{[8
]}

Schilke, P. ^{[9
]}

Urquhart, J. S. ^{[10
]}

Beltran, M. T. ^{[11
]}

Lumsden, S. L. ^{[12
]}

Leurini, S. ^{[13
]}

Moscadelli, L. ^{[11
]}

Cesaroni, R. ^{[11
]}

Sanchez-Monge, A. ^{[14
]}

Palau, A. ^{[15
]}

Pudritz, R. ^{[16
]}

Wyrowski, F. ^{[9
]}

Longmore, S. ^{[17
]}

机构：

[1] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany

[2] Univ Tubingen, Inst Astron & Astrophys, Morgenstelle 10, D-72076 Tubingen, Germany

[3] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands

[4] Domaine Univ, IRAM, 300 Rue Piscine, F-38406 St Martin Dheres, France

[5] Natl Astron Observ China, Datun Rd 20, Beijing, Peoples R China

[6] Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85748 Garching, Germany

[7] Ludwig Maximilians Univ Munchen, Dept Chem, Butenandtstr 5-13, D-81377 Munich, Germany

[8] Royal Observ Edinburgh, UK Astron Technol Ctr, Blackford Hill, Edinbugh EH9 3HJ, Scotland

[9] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany

[10] Univ Kent, Ctr Astrophys & Planetary Sci, Canterbury CT2 7NH, Kent, England

[11] INAF Osservatorio Astrofis Arcetri, Largo E Fermi 5, I-50125 Florence, Italy

[12] Univ Leeds, Sch Phys & Astron, Wood House Lane, Leeds LS2 9JT, W Yorkshire, England

[13] INAF Osservatorio Astron Cagliari, Via Sci 5, I-09047 Selargius, CA, Italy

[14] Univ Cologne, Phys Inst 1, Zulpicher Str 77, D-50937 Cologne, Germany

[15] Univ Nacl Autonoma Mexico, Inst Radioastron & Astrofis, POB 3-72, Morelia 58090, Michoacan, Mexico

[16] McMaster Univ, 1280 MAIN ST W, Hamilton, ON L8S 4M1, Canada

[17] Liverpool John Moores Univ, Astrophys Res Inst, 146 Brownlow Hill, Liverpool L3 5RF, Merseyside, England

[18] Heidelberg Univ, Max Planck Res Sch Astron & Cosm Phys, Heidelberg, Germany

[19] East Asian Core Observ Assoc, Heidelberg, Germany

来源：

ASTRONOMY & ASTROPHYSICS | 2019年 / 629卷

基金：

欧洲研究理事会;

关键词：

ISM: individual objects: IRAS 23033+5951; ISM: kinematics and dynamics; ISM: jets and outflows; circumstellar matter; stars: formation; stars: massive; PROTOSTELLAR CANDIDATES; MOLECULAR-SPECTROSCOPY; COLOGNE DATABASE; BIPOLAR FLOWS; H2O MASERS; ACCRETION; DISK; EMISSION; SIMULATIONS; EXCITATION;

D O I：

10.1051/0004-6361/201935318

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. The formation process of high-mass stars (>8 M-circle dot) is poorly constrained, particularly the effects of clump fragmentation creating multiple systems and the mechanism of mass accretion onto the cores. Aims. We study the fragmentation of dense gas clumps, and trace the circumstellar rotation and outflows by analyzing observations of the high-mass (similar to 500 M-circle dot) star-forming region IRAS 23033+5951. Methods. Using the Northern Extended Millimeter Array (NOEMA) in three configurations and the IRAM 30 m single-dish telescope at 220 GHz, we probe the gas and dust emission at an angular resolution of similar to 0.45 '', corresponding to 1900 au. Results. In the millimeter (mm) continuum emission, we identify a protostellar cluster with at least four mm-sources, where three of them show a significantly higher peak intensity well above a signal-to-noise ratio of 100. Hierarchical fragmentation from large to small spatial scales is discussed. Two fragments are embedded in rotating structures and drive molecular outflows, traced by (CO)-C-13 (2-1) emission. The velocity profiles across two of the cores are similar to Keplerian but are missing the highest-velocity components close to the center of rotation, which is a common phenomena from observations like these, and other rotation scenarios are not excluded entirely. Position-velocity diagrams suggest protostellar masses of similar to 6 and 19 M-circle dot. Rotational temperatures from fitting CH3CN (12(K)-11(K)) spectra are used for estimating the gas temperature and thereby also the disk stability against gravitational fragmentation, utilizing Toomre's Q parameter. Assuming that the candidate disk is in Keplerian rotation about the central stellar object and considering different disk inclination angles, we identify only one candidate disk as being unstable against gravitational instability caused by axisymmetric perturbations. Conclusions. The dominant sources cover different evolutionary stages within the same maternal gas clump. The appearance of rotation and outflows of the cores are similar to those found in low-mass star-forming regions.

引用

页数：23

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