The Gaia-ESO Survey: a kinematical and dynamical study of four young open clusters

被引：34

作者：

Bravi, L. ^{[1
,2
]}

Zari, E. ^{[3
]}

Sacco, G. G. ^{[2
]}

Randich, S. ^{[2
]}

Jeffries, R. D. ^{[4
]}

Jackson, R. J. ^{[4
]}

Franciosini, E. ^{[2
]}

Moraux, E. ^{[5
,6
]}

Lopez-Santiago, J. ^{[7
]}

Pancino, E. ^{[2
,8
]}

Spina, L. ^{[9
]}

Wright, N. ^{[4
]}

Jimenez-Esteban, F. M. ^{[10
]}

Klutsch, A. ^{[11
]}

Roccatagliata, V ^{[2
]}

Gilmore, G. ^{[12
]}

Bragaglia, A. ^{[13
]}

Flaccomio, E. ^{[14
]}

Francois, P. ^{[15
]}

Koposov, S. E. ^{[16
]}

Bayo, A. ^{[17
,18
]}

Carraro, G. ^{[19
]}

Costado, M. T. ^{[20
]}

Damiani, F. ^{[14
]}

Frasca, A. ^{[11
]}

Hourihane, A. ^{[11
]}

Jofre, P. ^{[21
]}

Lardo, C. ^{[22
]}

Lewis, J. ^{[12
]}

Magrini, L. ^{[2
]}

Morbidelli, L. ^{[2
]}

Prisinzano, L. ^{[14
]}

Sousa, S. G. ^{[23
]}

Worley, C. C. ^{[12
]}

Zaggia, S. ^{[24
]}

机构：

[1] Univ Florence, Dipartimento Fis & Astron, Via G Sansone 1, I-50019 Sesto Fiorentino, Firenze, Italy

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

[3] Leiden Observ, Niels Bohrweg 2, NL-2333 CA Leiden, Netherlands

[4] Keele Univ, Astrophys Grp, Keele ST5 5BG, Staffs, England

[5] Univ Grenoble Alpes, IPAG, CS 40700, F-38085 Grenoble 9, France

[6] CNRS, IPAG, F-38000 Grenoble, France

[7] Univ Carlos III Madrid, Dept Signal Theory & Commun, Madrid 28911, Spain

[8] ASI Space Sci Data Ctr, Via Politecn Snc, I-00133 Rome, Italy

[9] Univ Sao Paulo, Dept Astron, IAG, Rua Matao 1226, BR-05509900 Sao Paulo, SP, Brazil

[10] Ctr Astrobiol INTA CSIC, Dept Astrofis, ESAC Campus,Camino Bajo Castillo S-N, Madrid 28692, Spain

[11] INAF, Osservatorio Astrofis Catania, Via S Sofia 78, I-95123 Catania, Italy

[12] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England

[13] INAF Osservatorio Astrofis & Sci Spazio, Via Gobetti 93-3, I-40129 Bologna, Italy

[14] INAF Osservatorio Astron Palermo GS Vaiana, Piazza Parlamento 1, I-90134 Palermo, Italy

[15] Univ Paris Diderot, Observ Paris, CNRS, GEPI, 5 Pl Jules Janssen, F-92190 Meudon, France

[16] Carnegie Mellon Univ, McWilliams Ctr Cosmol, Dept Phys, 5000 Forbes Ave, Pittsburgh, PA 15213 USA

[17] Univ Valparaiso, Inst Fis & Astron, Valparaiso, Chile

[18] Univ Valparaiso, Millennium Nucleus Nucleo Planet Format, Valparaiso, Chile

[19] Univ Padua, Dipartimento Fis & Astron, Vicolo Osservatorio 3, I-35122 Padua, Italy

[20] Univ Cadiz, Dept Didact, Puerto Real 11519, Cadiz, Spain

[21] Univ Diego Portales, Fac Ingn, Nucleo Astron, Av Ejercito 441, Santiago, Chile

[22] EPFL, Lab Astrophys, Observ Sauverny, CH-1290 Versoix, Switzerland

[23] Univ Porto, Inst Astrofis & Ciencias Espaco, CAUP, Rua Estrelas, P-4150762 Porto, Portugal

[24] INAF Padova Observ, Vicolo Osservatorio 5, I-35122 Padua, Italy

来源：

ASTRONOMY & ASTROPHYSICS | 2018年 / 615卷

基金：

英国科学技术设施理事会; 欧盟地平线“2020”;

关键词：

stars: pre-main sequence; stars: kinematics and dynamics; open clusters and associations: general; stars: formation; techniques: spectroscopic; techniques: radial velocities; LOW-MASS STARS; SEQUENCE LITHIUM DEPLETION; GALACTIC OPEN CLUSTERS; SOLAR-TYPE STARS; IC; 2602; EMBEDDED CLUSTERS; GAS EXPULSION; BINARY STARS; TIDAL FIELDS; NGC; 2547;

D O I：

10.1051/0004-6361/201832645

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. The origin and dynamical evolution of star clusters is an important topic in stellar astrophysics. Several models have been proposed in order to understand the formation of bound and unbound clusters and their evolution, and they can be tested by examining the kinematical and dynamical properties of clusters over a wide range of ages and masses. Aims. We use the Gaia-ESO Survey products to study four open clusters (IC 2602, IC 2391, IC 4665, and NGC 2547) that lie in the age range between 20 and 50 Myr. Methods. We employ the gravity index gamma and the equivalent width of the lithium line at 6708 angstrom together with effective temperature T-eff and the metallicity of the stars in order to discard observed contaminant stars. Then we derive the cluster radial velocity dispersions sigma(c), the total cluster mass M-tot, and the half mass radius r(hm). Using the Gaia-DR1 TGAS catalogue, we independently derive the intrinsic velocity dispersion of the clusters from the astrometric parameters of cluster members. Results. The intrinsic radial velocity dispersions derived by the spectroscopic data are higher than those derived from the TGAS data, possibly due to the different masses of the considered stars. Using M-tot and r(hm) we derive the virial velocity dispersion sigma(vir) and we find that three out of four clusters are supervirial. This result is in agreement with the hypothesis that these clusters are dispersing, as predicted by the "residual gas expulsion" scenario. However, recent simulations show that the virial ratio of young star clusters may be overestimated if it is determined using the global velocity dispersion, since the clusters are not fully relaxed.

引用

页数：14

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