Core fragmentation and Toomre stability analysis of W3(H2O) A case study of the IRAM NOEMA large program CORE

被引：38

作者：

Ahmadi, A. ^{[1
,2
]}

Beuther, H. ^{[1
]}

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

Bosco, F. ^{[1
,2
]}

Linz, H. ^{[1
]}

Henning, Th ^{[1
]}

Winters, J. M. ^{[3
]}

Kuiper, R. ^{[4
]}

Pudritz, R. ^{[5
]}

Sanchez-Monge, A. ^{[6
]}

Keto, E. ^{[7
]}

Beltran, M. ^{[8
]}

Bontemps, S. ^{[9
]}

Cesaroni, R. ^{[8
]}

Csengeri, T. ^{[10
]}

Feng, S. ^{[11
]}

Galvan-Madrid, R. ^{[12
]}

Johnston, K. G. ^{[13
]}

Klaassen, P. ^{[14
]}

Leurini, S. ^{[15
]}

Longmore, S. N. ^{[16
]}

Lumsden, S. ^{[13
]}

Maud, L. T. ^{[17
]}

Menten, K. M. ^{[10
]}

Moscadelli, L. ^{[8
]}

Motte, F. ^{[18
]}

Palau, A. ^{[12
]}

Peters, T. ^{[19
]}

Ragan, S. E. ^{[20
]}

Schilke, P. ^{[6
]}

Urquhart, J. S. ^{[21
]}

Wyrowski, F. ^{[10
]}

Zinnecker, H. ^{[22
,23
]}

机构：

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

[2] Heidelberg Univ, Int Max Planck Res Sch Astron & Cosm Phys, IMPRS HD, Heidelberg, Germany

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

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

[5] McMaster Univ, Dept Phys & Astron, 1280 Main St W, Hamilton, ON L8S 4M1, Canada

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

[7] Harvard Smithsonian Ctr Astrophys, 160 Garden St, Cambridge, MA 02420 USA

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

[9] Univ Bordeaux 1, CNRS, UMR 5804, Lab Astrophys Bordeaux, F-33270 Floirac, France

[10] Max Planck Inst Radioastron, Hilgel 69, D-53121 Bonn, Germany

[11] Max Planck Inst Extraterr Phys, Gissenbachstr 1, D-85748 Garching, Germany

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

[13] Univ Leeds, Sch Phys & Astron, EC Stoner Bldg, Leeds LS2 9JT, W Yorkshire, England

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

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

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

[17] Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands

[18] Univ Grenoble Alpes, Inst Planetol & Astrophys Grenoble, CNRS, F-38000 Grenoble, France

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

[20] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales

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

[22] NASA, Ames Res Ctr, Deutsch SOFIA Inst, SOFIA Sci Ctr, Moffett Field, CA 94035 USA

[23] Univ Autonoma Chile, Av Pedro de Valdivia 425, Santiago, Chile

来源：

ASTRONOMY & ASTROPHYSICS | 2018年 / 618卷

基金：

欧洲研究理事会;

关键词：

stars: formation; stars: massive; stars: early-type; stars: kinematics and dynamics; stars: individual: W3(H2O)/(OH); techniques: interferometric; MASSIVE STAR-FORMATION; MOLECULAR CLOUD CORE; H2O MASER SOURCE; H-II REGIONS; GRAVITATIONAL-INSTABILITY; SYNCHROTRON EMISSION; CIRCUMSTELLAR DISKS; COLOGNE DATABASE; METHYL CYANIDE; ACCRETION;

D O I：

10.1051/0004-6361/201732548

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. The fragmentation mode of high-mass molecular clumps and the properties of the central rotating structures surrounding the most luminous objects have yet to be comprehensively characterised. Aims. We study the fragmentation and kinematics of the high-mass star-forming region W3(H2O), as part of the IRAM NOrthern Extended Millimeter Array (NOEMA) large programme CORE. Methods. Using the IRAM NOEMA and the IRAM 30 m telescope, the CORE survey has obtained high-resolution observations of 20 well-known highly luminous star-forming regions in the 1.37 mm wavelength regime in both line and dust continuum emission. Results. We present the spectral line setup of the CORE survey and a case study for W3(H2O). At similar to 0 ''.35 (700 AU at 2.0 kpc) resolution, the W3(H2O) clump fragments into two cores (west and east), separated by similar to 2300 AU. Velocity shifts of a few km s(-1) are observed in the dense-gas tracer, CH3CN, across both cores, consistent with rotation and perpendicular to the directions of two bipolar outflows, one emanating from each core. The kinematics of the rotating structure about W3(H2O) W shows signs of differential rotation of material, possibly in a disk-like object. The observed rotational signature around W3(H2O) E may be due to a disk-like object, an unresolved binary (or multiple) system, or a combination of both. We fit the emission of CH3CN (12(K) -11 (K)), K = 4-6 and derive a gas temperature map with a median temperature of similar to 165 K across W3(H2O). We create a Toomre Q map to study the stability of the rotating structures against gravitational instability. The rotating structures appear to be Toomre unstable close to their outer boundaries, with a possibility of further fragmentation in the differentially rotating core, W3(H2O) W. Rapid cooling in the Toomre unstable regions supports the fragmentation scenario. Conclusions. Combining millimetre dust continuum and spectral line data toward the famous high-mass star-forming region W3(H2O), we identify core fragmentation on large scales, and indications for possible disk fragmentation on smaller spatial scales.

引用

页数：22

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