The Tarantula Massive Binary Monitoring I. Observational campaign and OB-type spectroscopic binaries

被引：111

作者：

Almeida, L. A. ^{[1
,2
]}

Sana, H. ^{[3
,4
]}

Taylor, W. ^{[5
]}

Barba, R. ^{[6
]}

Bonanos, A. Z. ^{[7
]}

Crowther, P. ^{[8
]}

Damineli, A. ^{[1
]}

de Koter, A. ^{[3
,9
]}

de Mink, S. E. ^{[9
]}

Evans, C. J. ^{[5
]}

Gieles, M. ^{[10
]}

Grin, N. J. ^{[12
]}

Henault-Brunet, V. ^{[11
]}

Langer, N. ^{[12
]}

Lennon, D. ^{[13
]}

Lockwood, S. ^{[4
]}

Maiz Apellaniz, J. ^{[14
]}

Moffat, A. F. J. ^{[15
,16
]}

Neijssel, C. ^{[9
]}

Norman, C. ^{[2
]}

Ramirez-Agudelo, O. H. ^{[5
]}

Richardson, N. D. ^{[17
]}

Schootemeijer, A. ^{[12
]}

Shenar, T. ^{[18
]}

Soszynski, I. ^{[19
]}

Tramper, F. ^{[13
]}

Vink, J. S. ^{[20
]}

机构：

[1] Inst Astron Geofis & Ciencias Atmosfer, Rua Matao 1226, BR-05508090 Sao Paulo, SP, Brazil

[2] Johns Hopkins Univ, Dept Phys & Astron, Bloomberg Ctr Phys & Astron, Room 520,3400 N Charles St, Baltimore, MD 21218 USA

[3] Katholieke Univ Leuven, Inst Astrophys, Celestijnenlaan 200 D, B-3001 Leuven, Belgium

[4] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA

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

[6] Univ La Serena, Dept Fis & Astron, Av Cisternas 1200 Norte, La Serena, Chile

[7] Natl Observ Athens, IAASARS, Penteli 15326, Greece

[8] Univ Sheffield, Dept Phys & Astron, Housnsfield Rd, Sheffield S3 7RH, S Yorkshire, England

[9] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands

[10] Univ Surrey, Dept Phys, Guildford GU2 7XH, Surrey, England

[11] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, POB 9010, NL-6500 GL Nijmegen, Netherlands

[12] Univ Bonn, Argelander Inst Astron, Hugel 71, D-53121 Bonn, Germany

[13] European Space Astron Ctr ESA ESAC, POB 78, Madrid 28691, Spain

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

[15] Univ Montreal, Dept Phys, CP 6128,Succ C-V, Montreal, PQ H3C 3J7, Canada

[16] Ctr Rech Astrophys Quebec, CP 6128,Succ C-V, Montreal, PQ H3C 3J7, Canada

[17] Univ Toledo, Dept Phys & Astron, Ritter Observ, 2801 W Bancroft St, Toledo, OH 43606 USA

[18] Univ Potsdam, Inst Phys & Astron, Karl Liebknecht Str 24-25, D-14476 Potsdam, Germany

[19] Univ Warsaw Observ, Al Ujazdowskie 4, PL-00478 Warsaw, Poland

[20] Armagh Observ, Coll Hill, Armagh BT61 9DG, North Ireland

来源：

ASTRONOMY & ASTROPHYSICS | 2017年 / 598卷

基金：

美国国家科学基金会; 欧盟地平线“2020”; 巴西圣保罗研究基金会; 加拿大自然科学与工程研究理事会; 欧洲研究理事会;

关键词：

stars: early-type; stars: massive; binaries: spectroscopic; binaries: close; GRAVITATIONAL LENSING EXPERIMENT; CYGNUS OB2; INTERACTING BINARIES; STELLAR POPULATIONS; MAIN-SEQUENCE; SPACED DATA; GALACTIC O; 30; DORADUS; STARS; EVOLUTION;

D O I：

10.1051/0004-6361/201629844

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. Massive binaries play a crucial role in the Universe. Knowing the distributions of their orbital parameters is important for a wide range of topics from stellar feedback to binary evolution channels and from the distribution of supernova types to gravitational wave progenitors, yet no direct measurements exist outside the Milky Way. Aims. The Tarantula Massive Binary Monitoring project was designed to help fill this gap by obtaining multi-epoch radial velocity (RV) monitoring of 102 massive binaries in the 30 Doradus region. Methods. In this paper we analyze 32 FLAMES/GIRAFFE observations of 93 O- and 7 B-type binaries. We performed a Fourier analysis and obtained orbital solutions for 82 systems: 51 single-lined (SB1) and 31 double-lined (SB2) spectroscopic binaries. Results. Overall, the binary fraction and orbital properties across the 30 Doradus region are found to be similar to existing Galactic samples. This indicates that within these domains environmental effects are of second order in shaping the properties of massive binary systems. A small difference is found in the distribution of orbital periods, which is slightly flatter (in log space) in 30 Doradus than in the Galaxy, although this may be compatible within error estimates and differences in the fitting methodology. Also, orbital periods in 30 Doradus can be as short as 1.1 d, somewhat shorter than seen in Galactic samples. Equal mass binaries (q > 0.95) in 30 Doradus are all found outside NGC 2070, the central association that surrounds R136a, the very young and massive cluster at 30 Doradus's core. Most of the differences, albeit small, are compatible with expectations from binary evolution. One outstanding exception, however, is the fact that earlier spectral types (O2-O7) tend to have shorter orbital periods than later spectral types (O9.2-O9.7). Conclusions. Our results point to a relative universality of the incidence rate of massive binaries and their orbital properties in the metallicity range from solar (Z(circle dot)) to about half solar. This provides the first direct constraints on massive binary properties in massive star-forming galaxies at the Universe's peak of star formation at redshifts z similar to 1 to 2 which are estimated to have Z similar to 0.5 Z(circle dot).

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