Binarity at LOw Metallicity (BLOeM) A spectroscopic VLT monitoring survey of massive stars in the SMC

被引：5

作者：

Shenar, T. ^{[1
]}

Bodensteiner, J. ^{[2
]}

Sana, H. ^{[3
]}

Crowther, P. A. ^{[4
]}

Lennon, D. J. ^{[5
,6
]}

Abdul-Masih, M. ^{[5
,6
]}

Almeida, L. A. ^{[7
]}

Backs, F. ^{[3
]}

Berlanas, S. R. ^{[5
,6
]}

Bernini-Peron, M. ^{[8
]}

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

Bowman, D. M. ^{[3
,9
]}

Bronner, V. A. ^{[10
,11
]}

Britavskiy, N. ^{[12
]}

de Koter, A. ^{[3
,13
]}

de Mink, S. E. ^{[14
]}

Deshmukh, K. ^{[3
]}

Evans, C. J. ^{[15
]}

Fabry, M. ^{[3
]}

Gieles, M. ^{[16
,17
]}

Gilkis, A. ^{[18
]}

Gonzalez-Tora, G. ^{[8
]}

Graefener, G. ^{[19
]}

Goetberg, Y. ^{[20
]}

Hawcroft, C. ^{[21
]}

Henault-Brunet, V. ^{[22
]}

Herrero, A. ^{[5
,6
]}

Holgado, G. ^{[5
,6
]}

Janssens, S. ^{[3
]}

Johnston, C. ^{[3
,14
]}

Josiek, J. ^{[8
]}

Justham, S. ^{[14
]}

Kalari, V. M. ^{[23
]}

Katabi, Z. Z. ^{[1
]}

Keszthelyi, Z. ^{[24
]}

Klencki, J. ^{[2
]}

Kubat, J. ^{[25
]}

Kubatova, B. ^{[25
]}

Langer, N. ^{[19
]}

Lefever, R. R. ^{[8
]}

Ludwig, B. ^{[26
]}

Mackey, J. ^{[27
]}

Mahy, L. ^{[12
]}

Maiz Apellaniz, J. ^{[28
]}

Mandel, I. ^{[29
,30
]}

Maravelias, G. ^{[31
,32
]}

Marchant, P. ^{[3
]}

Menon, A. ^{[5
,6
]}

Najarro, F. ^{[33
]}

Oskinova, L. M. ^{[34
]}

机构：

[1] Tel Aviv Univ, Sch Phys & Astron, IL-6997801 Tel Aviv, Israel

[2] ESO European Southern Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany

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

[4] Univ Sheffield, Dept Phys & Astron, Hounsfield Rd, Sheffield S3 7RH, England

[5] Inst Astrofis Canarias, C Via Lactea S-N, E-38200 San Cristobal la Laguna, Santa Cruz De T, Spain

[6] Univ La Laguna, Dept Astrofis, Ave Astrofis Francisco Sanchez, San Cristobal la Laguna 38206, Santa Cruz De T, Spain

[7] Univ Fed Rio Grande do Norte, Escola Ciencias & Tecnol, BR-59072970 Natal, RN, Brazil

[8] Heidelberg Univ, Astron Rechen Inst, Zentrum Astron, Monchhofstr 12-14, D-69120 Heidelberg, Germany

[9] Newcastle Univ, Sch Math Stat & Phys, Newcastle Upon Tyne NE1 7RU, England

[10] Heidelberger Inst Theoret Studien, Schloss Wolfsbrunnenweg 35, D-69118 Heidelberg, Germany

[11] Heidelberg Univ, Dept Phys & Astron, Neuenheimer Feld 226, D-69120 Heidelberg, Germany

[12] Royal Observ Belgium, Ave Circulaire Ringlaan 3, B-1180 Brussels, Belgium

[13] Univ Amsterdam, Anton Pannekoek Inst Astron, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands

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

[15] European Space Agcy ESA, Space Telescope Sci Inst, ESA Off, 3700 San Martin Dr, Baltimore, MD 21218 USA

[16] ICREA, Pg Lluis Co 23, Barcelona 08010, Spain

[17] Univ Barcelona IEEC UB, Inst Ciencies Cosmos ICCUB, Marti i Franques 1, 08028 Barcelona, Spain

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

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

[20] Inst Sci & Technol Austria ISTA, Campus 1, A-3400 Klosterneuburg, Austria

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

[22] St Marys Univ, Dept Astron & Phys, 923 Robie St, Halifax, NS B3H 3C3, Canada

[23] Gemini Observ NSFs NOIRLab, Casilla 603, La Serena, Chile

[24] Natl Astron Observ Japan, Ctr Computat Astrophys, Div Sci, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan

[25] Acad Sci Czech Republ, Astron Inst, Fricova 298, CZ-25165 Ondrejov, Czech Republic

[26] Univ Toronto, Dept Astron & Astrophys, 50 St George St, Toronto, ON M5S 3H4, Canada

[27] Dublin Inst Adv Studies, DIAS Dunsink Observ, Astrophys Sect, Dunsink Lane, Dublin 15, Ireland

[28] Ctr Astrobiol CSIC INTA, Campus ESAC,Camino Bajo Castillo S-n, Villanueva De La Canada 28692, Spain

[29] Monash Univ, Sch Phys & Astron, Clayton, Vic 3800, Australia

[30] ARC Ctr Excellence Gravitat wave Discovery OzGrav, Melbourne, Australia

[31] Natl Observ Athens, IAASARS, Penteli 15236, Greece

[32] FORTH, Inst Astrophys, Iraklion 71110, Greece

[33] Ctr Astrobiol CSIC INTA, Ctra Torrejon Ajalvir Km 4, Torrejon De Ardoz 28850, Spain

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

[35] Carnegie Mellon Univ, McWilliams Ctr Cosmol & Astrophys, Dept Phys, Pittsburgh, PA 15213 USA

[36] Lund Univ, Dept Phys, Div Astrophys, Lund Observ, Box 43, S-22100 Lund, Sweden

[37] Dept Astron, 933 N Cherry Ave, Tucson, AZ 85721 USA

[38] Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA

[39] Observ Nacl, R Gen Jose Cristino,77 Vasco Da Gama, BR-20921400 Rio De Janeiro, RJ, Brazil

[40] Nicolaus Copernicus Univ, Inst Astron, Fac Phys Astron & Informat, Grudziadzka 5, PL-87100 Torun, Poland

[41] Weizmann Inst Sci, Dept Particle Phys & Astrophys, IL-7610001 Rehovot, Israel

[42] Keele Univ, Lennard Jones Labs, Keele ST5 5BG, Staffs, England

[43] Flatiron Inst, Ctr Computat Astrophys, New York, NY 10010 USA

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

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

来源：

ASTRONOMY & ASTROPHYSICS | 2024年 / 690卷

基金：

欧洲研究理事会; 英国科学技术设施理事会; 英国科研创新办公室; 爱尔兰科学基金会; 澳大利亚研究理事会;

关键词：

binaries: general; binaries: spectroscopic; stars: massive; Magellanic Clouds; SMALL-MAGELLANIC-CLOUD; BLANKETED MODEL ATMOSPHERES; WOLF-RAYET STARS; BLACK-HOLE CANDIDATE; B-TYPE STARS; MULTIPLICITY PROPERTIES; STELLAR MERGERS; OB STARS; SPECTRAL CLASSIFICATION; OBSERVATIONAL CAMPAIGN;

D O I：

10.1051/0004-6361/202451586

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Surveys in the Milky Way and Large Magellanic Cloud have revealed that the majority of massive stars will interact with companions during their lives. However, knowledge of the binary properties of massive stars at low metallicity, and therefore in conditions approaching those of the Early Universe, remain sparse. We present the Binarity at LOw Metallicity (BLOeM) campaign, an ESO large programme designed to obtain 25 epochs of spectroscopy for 929 massive stars in the Small Magellanic Cloud, allowing us to probe multiplicity in the lowest-metallicity conditions to date (Z = 0.2 Z circle dot). BLOeM will provide (i) the binary fraction, (ii) the orbital configurations of systems with periods of P less than or similar to 3 yr, (iii) dormant black-hole binary candidates (OB+BH), and (iv) a legacy database of physical parameters of massive stars at low metallicity. Main sequence (OB-type) and evolved (OBAF-type) massive stars are observed with the LR02 setup of the GIRAFFE instrument of the Very Large Telescope (3960-4570 & Aring; resolving power R = 6200; typical signal-to-noise ratio(S/N) approximate to 70-100). This paper utilises the first nine epochs obtained over a three-month time period. We describe the survey and data reduction, perform a spectral classification of the stacked spectra, and construct a Hertzsprung-Russell diagram of the sample via spectral-type and photometric calibrations. Our detailed classification reveals that the sample covers spectral types from O4 to F5, spanning the effective temperature and luminosity ranges 6.5 less than or similar to Teff/kK less than or similar to 45 and 3.7 < log L/L-circle dot < 6.1 and initial masses of 8 less than or similar to Mini less than or similar to 80 M-circle dot. The sample comprises 159 O-type stars, 331 early B-type (B0-3) dwarfs and giants (luminosity classes V-III), 303 early B-type supergiants (II-I), and 136 late-type BAF supergiants. At least 82 stars are OBe stars: 20 O-type and 62 B-type (13% and 11% of the respective samples). In addition, the sample includes 4 high-mass X-ray binaries, 3 stars resembling luminous blue variables, 2 bloated stripped-star candidates, 2 candidate magnetic stars, and 74 eclipsing binaries.

引用

页数：22

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