The GALAH plus survey: Third data release

被引：440

作者：

Buder, Sven ^{[1
,2
,3
]}

Sharma, Sanjib ^{[2
,4
]}

Kos, Janez ^{[5
]}

Amarsi, Anish M. ^{[6
]}

Nordlander, Thomas ^{[1
,2
]}

Lind, Karin ^{[3
,7
]}

Martell, Sarah L. ^{[2
,8
]}

Asplund, Martin ^{[9
]}

Bland-Hawthorn, Joss ^{[2
,4
]}

Casey, Andrew R. ^{[10
,11
]}

De Silva, Gayandhi M. ^{[12
,13
]}

D'Orazi, Valentina ^{[14
]}

Freeman, Ken C. ^{[1
,2
]}

Hayden, Michael R. ^{[2
,4
]}

Lewis, Geraint F. ^{[4
]}

Lin, Jane ^{[1
,2
]}

Schlesinger, Katharine J. ^{[1
]}

Simpson, Jeffrey D. ^{[2
,8
]}

Stello, Dennis ^{[4
,8
,15
]}

Zucker, Daniel B. ^{[13
,16
]}

Zwitter, Tomaz ^{[5
]}

Beeson, Kevin L. ^{[5
]}

Buck, Tobias ^{[17
]}

Casagrande, Luca ^{[1
,2
]}

Clark, Jake T. ^{[18
]}

Cotar, Klemen ^{[5
]}

Da Costa, Gary S. ^{[1
,2
]}

de Grijs, Richard ^{[13
,16
,19
]}

Feuillet, Diane ^{[3
,20
]}

Horner, Jonathan ^{[18
]}

Kafle, Prajwal R. ^{[21
]}

Khanna, Shourya ^{[22
]}

Kobayashi, Chiaki ^{[2
,23
]}

Liu, Fan ^{[24
]}

Montet, Benjamin T. ^{[8
]}

Nandakumar, Govind ^{[1
,2
]}

Nataf, David M. ^{[25
,26
]}

Ness, Melissa K. ^{[27
,28
]}

Spina, Lorenzo ^{[2
,11
,14
]}

Tepper-Garcia, Thor ^{[2
,4
,29
]}

Ting, Yuan-Sen ^{[1
,30
,31
,32
]}

Traven, Gregor ^{[20
]}

Vogrincic, Rok ^{[5
]}

Wittenmyer, Robert A. ^{[18
]}

Wyse, Rosemary F. G. ^{[25
,26
]}

Zerjal, Marusa ^{[1
]}

机构：

[1] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia

[2] Ctr Excellence Astrophys Three Dimens ASTRO 3D, Melbourne, Vic, Australia

[3] Max Planck Inst Astron MPIA, Koenigstuhl 17, D-69117 Heidelberg, Germany

[4] Univ Sydney, Sch Phys, Sydney Inst Astron, A28, Sydney, NSW 2006, Australia

[5] Univ Ljubljana, Fac Math & Phys, Jadranska 19, Ljubljana 1000, Slovenia

[6] Uppsala Univ, Dept Phys & Astron, Theoret Astrophys, Box 516, SE-75120 Uppsala, Sweden

[7] Stockholm Univ, Dept Astron, AlbaNova, Roslagstullbacken 11, SE-75120 Stockholm, Sweden

[8] UNSW, Sch Phys, Sydney, NSW 2052, Australia

[9] Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85741 Garching, Germany

[10] Monash Univ, Monash Ctr Astrophys, Wellington Rd, Clayton, Vic 3800, Australia

[11] Monash Univ, Sch Phys & Astron, Wellington Rd, Clayton, Vic 3800, Australia

[12] Macquarie Univ, Fac Sci & Engn, Australian Astron Opt, Macquarie Pk, NSW 2113, Australia

[13] Macquarie Univ, Dept Phys & Astron, Sydney, NSW 2109, Australia

[14] Ist Nazl Astrofis, Osservatorio Astron Padova, Vicolo Osservatorio 5,1, I-35122 Padua, Italy

[15] Aarhus Univ, Stellar Astrophys Ctr, Dept Phys & Astron, Ny Munkegade 120, DK-8000 Aarhus C, Denmark

[16] Macquarie Univ, Res Ctr Astron Astrophys Astrophoton, Sydney, NSW 2109, Australia

[17] Leibniz Inst Astrophys Potsdam AIP, Sternwarte 16, D-14482 Potsdam, Germany

[18] Univ Southern Queensland, Ctr Astrophys, West St, Toowoomba, Qld 4350, Australia

[19] Int Space Sci Inst Beijing, 1 Nanertiao, Beijing 100190, Peoples R China

[20] Dept Astron & Theoret Phys, Lund Observ, Box 43, SE-22100 Lund, Sweden

[21] Univ Western Australia, ICRAR, 35 Stirling Highway, Crawley, WA 6009, Australia

[22] Univ Groningen, Kapteyn Astron Inst, Landleven 12, NL-9747 AD Groningen, Netherlands

[23] Univ Hertfordshire, Dept Phys Astron & Math, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England

[24] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia

[25] Johns Hopkins Univ, Ctr Astrophys Sci, Baltimore, MD 21218 USA

[26] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA

[27] Columbia Univ, Dept Astron, Pupin Phys Labs, New York, NY 10027 USA

[28] Flatiron Inst, Ctr Computat Astrophys, 162 Fifth Av, New York, NY 10010 USA

[29] Univ Sydney, Sch Phys, Ctr Integrated Sustainabil Anal, Sydney, NSW 2006, Australia

[30] Inst Adv Study, Princeton, NJ 08540 USA

[31] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA

[32] Observ Carnegie Inst Washington, 813 Santa Barbara St, Pasadena, CA 91101 USA

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2021年 / 506卷 / 01期

基金：

欧洲研究理事会; 澳大利亚研究理事会; 英国科学技术设施理事会; 美国国家航空航天局; 瑞典研究理事会; 美国国家科学基金会;

关键词：

methods: data analysis; methods: observational; surveys; stars: abundances; stars: fundamental parameters; RELATIVE OSCILLATOR-STRENGTHS; LABORATORY TRANSITION-PROBABILITIES; FGK BENCHMARK STARS; GAIA-ESO SURVEY; PLANET-CANDIDATE PROPERTIES; DISTINCT HALO POPULATIONS; LTE LINE FORMATION; FE-I TRANSITIONS; RED GIANT STARS; R-PROCESS-RICH;

D O I：

10.1093/mnras/stab1242

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The ensemble of chemical element abundance measurements for stars, along with precision distances and orbit properties, provides high-dimensional data to study the evolution of the Milky Way. With this third data release of the Galactic Archaeology with HERMES (GALAH) survey, we publish 678 423 spectra for 588 571 mostly nearby stars (81.2 per cent of stars are within <2 kpc), observed with the HERMES spectrograph at the Anglo-Australian Telescope. This release (hereafter GALAH+ DR3) includes all observations from GALAH Phase 1 (bright, main, and faint survey, 70 per cent), K2-HERMES (17 per cent), TESS-HERMES (5 per cent), and a subset of ancillary observations (8 per cent) including the bulge and >75 stellar clusters. We derive stellar parameters T-eff, logg, [Fe/H], v(mic), v(broad), and v(rad) using our modified version of the spectrum synthesis code Spectroscopy Made Easy (SME) and 1D MARCS model atmospheres. We break spectroscopic degeneracies in our spectrum analysis with astrometry from Gaia DR2 and photometry from 2MASS. We report abundance ratios [X/Fe] for 30 different elements (11 of which are based on non-LTE computations) covering five nucleosynthetic pathways. We describe validations for accuracy and precision, flagging of peculiar stars/measurements and recommendations for using our results. Our catalogue comprises 65 per cent dwarfs, 34 per cent giants, and 1 per cent other/unclassified stars. Based on unflagged chemical composition and age, we find 62 per cent young low-alpha, 9 per cent young high-alpha, 27 per cent old high-alpha, and 2 per cent stars with [Fe/H] <= -1. Based on kinematics, 4 per cent are halo stars. Several Value-Added-Catalogues, including stellar ages and dynamics, updated after Gaia eDR3, accompany this release and allow chrono-chemodynamic analyses, as we showcase.

引用

页码：150 / 201

页数：52

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