The Gaia-ESO survey: A spectroscopic study of the young open cluster NGC 3293

被引：8

作者：

Morel, T. ^{[1
]}

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

Semaan, T. ^{[1
,3
]}

Gosset, E. ^{[1
]}

Zorec, J. ^{[4
]}

Fremat, Y. ^{[5
]}

Blomme, R. ^{[5
]}

Daflon, S. ^{[6
]}

Lobel, A. ^{[5
]}

Nieva, M. F. ^{[7
]}

Przybilla, N. ^{[7
]}

Gebran, M. ^{[8
,9
]}

Herrero, A. ^{[10
,11
]}

Mahy, L. ^{[1
,5
,12
]}

Santos, W. ^{[6
]}

Tautvaisiene, G. ^{[13
]}

Gilmore, G. ^{[14
]}

Randich, S. ^{[15
]}

Alfaro, E. J. ^{[20
]}

Bergemann, M. ^{[17
,18
]}

Carraro, G. ^{[22
]}

Damiani, F. ^{[16
]}

Franciosini, E. ^{[15
]}

Morbidelli, L. ^{[15
]}

Pancino, E. ^{[15
,21
]}

Worley, C. C. ^{[14
]}

Zaggia, S. ^{[19
]}

机构：

[1] Univ Liege, Space Sci Technol & Astrophys Res STAR Inst, Allee 6 Aout 19c, B-4000 Liege, Belgium

[2] Ctr Natl Etud Spatiales, Toulouse, France

[3] Univ Geneva, Observ Geneve, Chemin Pegasi 51, CH-1290 Versoix, Switzerland

[4] Sorbonne Univ, Inst Astrophys Paris, CNRS, UMR 7095, F-75014 Paris, France

[5] Royal Observ Belgium, Ringlaan 3, B-1180 Brussels, Belgium

[6] Observ Nacl MCTIC, R Gal Jose Cristino 77, BR-20921400 Rio De Janeiro 20921400, RJ, Brazil

[7] Univ Innsbruck, Inst Astro & Teilchenphys, Technikerstr 25-8, A-6020 Innsbruck, Austria

[8] Notre Dame Univ Louaize, Dept Phys & Astron, POB 72, Zouk Mikael, Lebanon

[9] St Marys Coll, Dept Chem & Phys, Notre Dame, IN 46556 USA

[10] Inst Astrofis Canarias, Tenerife 38205, Spain

[11] Univ La Laguna, Dept Astrofis, Tenerife 38206, Spain

[12] Katholieke Univ Leuven, Inst Astron, Celestijnenlaan 200D, B-3001 Leuven, Belgium

[13] Vilnius Univ, Inst Theoret Phys & Astron, Sauletekio Av 3, LT-10257 Vilnius, Lithuania

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

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

[16] INAF Osservatorio Astron Palermo, Piazza Parlamento 1, I-90134 Palermo, Italy

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

[18] Univ Copenhagen, Niels Bohr Int Acad, Niels Bohr Inst, Blegdamsvej 17, DK-2100 Copenhagen, Denmark

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

[20] CSIC, Inst Astrofis Andalucia, Apdo 3004, Granada 18080, Spain

[21] Agenzia Spaziale Italiana, Space Sci Data Ctr, Via Politecn Snc, I-00133 Rome, Italy

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

来源：

ASTRONOMY & ASTROPHYSICS | 2022年 / 665卷

基金：

欧洲研究理事会; 奥地利科学基金会; 欧盟地平线“2020”;

关键词：

open clusters and associations: individual: NGC 3293; stars: fundamental parameters; stars: abundances; B-TYPE STARS; VLT-FLAMES SURVEY; FOSSIL MAGNETIC-FIELDS; M-CIRCLE-DOT; SURVEY MEMBERSHIP PROBABILITIES; BLANKETED MODEL ATMOSPHERES; MAIN-SEQUENCE TURNOFFS; BETA-CEPHEI STARS; MASSIVE STARS; ROTATIONAL VELOCITIES;

D O I：

10.1051/0004-6361/202244112

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present a spectroscopic analysis of the GIRAFFE and UVES data collected by the Gaia-ESO survey for the young open cluster NGC 3293. Archive spectra from the same instruments obtained in the framework of the 'VLT-FLAMES survey of massive stars' are also analysed. Atmospheric parameters, non-local thermodynamic equilibrium (LTE) chemical abundances for six elements (He, C, N, Ne, Mg, and Si), or variability information are reported for a total of about 160 B stars spanning a wide range in terms of spectral types (B1 to B9.5) and rotation rate (up to 350 km s(-1)). Our analysis leads to about a five-fold increase in the number of cluster members with an abundance determination and it characterises the late B-star population in detail for the first time. We take advantage of the multi-epoch observations on various timescales and a temporal baseline, sometimes spanning similar to 15 years, to detect several binary systems or intrinsically line-profile variables. A deconvolution algorithm is used to infer the current, true (deprojected) rotational velocity distribution. We find a broad, Gaussian-like distribution peaking around 200-250 km s(-1). Although some stars populate the high-velocity tail, most stars in the cluster appear to rotate far from critical. We discuss the chemical properties of the cluster, including the low occurrence of abundance peculiarities in the late B stars and the paucity of objects showing CN-cycle burning products at their surface. We argue that the former result can largely be explained by the inhibition of diffusion effects because of fast rotation, while the latter is generally in accord with the predictions of single-star evolutionary models under the assumption of a wide range of initial spin rates at the onset of main-sequence evolution. However, we find some evidence for a less efficient mixing in two quite rapidly rotating stars that are among the most massive objects in our sample. Finally, we obtain a cluster age of similar to 20 Myr through a detailed, star-to-star correction of our results for the effect of stellar rotation (e.g., gravity darkening). This is significantly older than previous estimates from turn-off fitting that fully relied on classical, non-rotating isochrones.

引用

页数：29

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