Chemical Abundance Analysis of Tucana III, the Second r-process Enhanced Ultra-faint Dwarf Galaxy

被引：41

作者：

Marshall, J. L. ^{[1
,2
]}

Hansen, T. ^{[3
]}

Simon, J. D. ^{[3
]}

Li, T. S. ^{[4
]}

Bernstein, R. A. ^{[3
]}

Kuehn, K. ^{[5
]}

Pace, A. B. ^{[1
,2
]}

DePoy, D. L. ^{[1
,2
]}

Palmese, A. ^{[4
]}

Pieres, A. ^{[6
]}

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

Drlica-Wagner, A. ^{[4
]}

Bechtol, K. ^{[7
,8
]}

Lidman, C. ^{[9
]}

Nagasawa, D. Q. ^{[1
,2
]}

Bertin, E. ^{[10
,11
]}

Brooks, D. ^{[12
]}

Buckley-Geer, E. ^{[4
]}

Burke, D. L. ^{[13
,14
]}

Rosell, A. Carnero ^{[6
,15
]}

Kind, M. Carrasco ^{[16
,17
]}

Carretero, J. ^{[18
]}

Cunha, C. E. ^{[13
]}

D'Andrea, C. B. ^{[19
]}

da Costa, L. N. ^{[6
,20
]}

De Vicente, J. ^{[15
]}

Desai, S. ^{[21
]}

Doel, P. ^{[12
]}

Eifler, T. F. ^{[22
,23
]}

Flaugher, B. ^{[4
]}

Fosalba, P. ^{[24
,25
]}

Frieman, J. ^{[4
,26
]}

Garcia-Bellido, J. ^{[27
]}

Gaztanaga, E. ^{[24
,25
]}

Gerdes, D. W. ^{[28
,29
]}

Gruendl, R. A. ^{[16
,17
]}

Gschwend, J. ^{[6
,20
]}

Gutierrez, G. ^{[4
]}

Hartley, W. G. ^{[12
,30
]}

Hollowood, D. L. ^{[31
]}

Honscheid, K. ^{[32
,33
]}

Hoyle, B. ^{[34
,35
]}

James, D. J. ^{[36
]}

Kuropatkin, N. ^{[4
]}

Maia, M. A. G. ^{[6
,20
]}

Menanteau, F. ^{[16
,17
]}

Miller, C. J. ^{[28
,29
]}

Miquel, R. ^{[18
,37
]}

Plazas, A. A. ^{[23
]}

Sanchez, E. ^{[15
]}

机构：

[1] Texas A&M Univ, Mitchell Inst Fundamental Phys & Astron, College Stn, TX 77843 USA

[2] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA

[3] Carnegie Inst Sci, 813 Santa Barbara St, Pasadena, CA 91101 USA

[4] Fermilab Natl Accelerator Lab, POB 500, Batavia, IL 60510 USA

[5] Macquarie Univ, Australian Astron Opt, N Ryde, NSW 2113, Australia

[6] Lab Interinst & Astron LIneA, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil

[7] LSST, 933 North Cherry Ave, Tucson, AZ 85721 USA

[8] Univ Wisconsin, Phys Dept, 2320 Chamberlin Hall,1150 Univ Ave, Madison, WI 53706 USA

[9] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2601, Australia

[10] Inst Astrophys Paris, CNRS, UMR 7095, F-75014 Paris, France

[11] Sorbonne Univ, UPMC Univ Paris 06, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France

[12] UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England

[13] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, POB 2450, Stanford, CA 94305 USA

[14] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA

[15] Ctr Invest Energet Medioambientales & Tecnol CIEM, Madrid, Spain

[16] Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA

[17] Natl Ctr Supercomp Applicat, 1205 West Clark St, Urbana, IL 61801 USA

[18] Barcelona Inst Sci & Technol, IFAE, Campus UAB, E-08193 Bellaterra, Barcelona, Spain

[19] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA

[20] Observ Nacl, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil

[21] IIT Hyderabad, Dept Phys, Kandi 502285, Telangana, India

[22] Steward Observ, Dept Astron, 933 North Cherry Ave, Tucson, AZ 85721 USA

[23] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA

[24] IEEC, E-08034 Barcelona, Spain

[25] CSIC, Inst Space Sci ICE, Campus UAB,Caner Can Magrans S-N, E-08193 Barcelona, Spain

[26] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA

[27] Univ Autonoma Madrid, Inst Fis Teor, CSIC, E-28049 Madrid, Spain

[28] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA

[29] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA

[30] Swiss Fed Inst Technol, Dept Phys, Wolfgang Pauli Str 16, CH-8093 Zurich, Switzerland

[31] Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA

[32] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA

[33] Ohio State Univ, Dept Phys, 174 W 18th Ave, Columbus, OH 43210 USA

[34] Max Planck Inst Extraterr Phys, Giessenbachstr, D-85748 Garching, Germany

[35] Ludwig Maximilians Univ Munchen, Univ Sternwarte, Fak Phys, Scheinerstr 1, D-81679 Munich, Germany

[36] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA

[37] Inst Catalana Recerca & Estudis Avancats, E-08010 Barcelona, Spain

[38] Univ Fed Rio Grande do Sul, Inst Fis, Caixa Postal 15051, BR-91501970 Porto Alegre, RS, Brazil

[39] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England

[40] Brandeis Univ, Phys Dept, 415 South St, Waltham, MA 02453 USA

[41] Oak Ridge Natl Lab, Comp Sci & Math Div, POB 2009, Oak Ridge, TN 37831 USA

来源：

ASTROPHYSICAL JOURNAL | 2019年 / 882卷 / 02期

基金：

美国国家科学基金会; 澳大利亚研究理事会; 欧洲研究理事会; 英国科学技术设施理事会;

关键词：

METAL-POOR STARS; HIGH-RESOLUTION SPECTROSCOPY; EVOLUTION; ELEMENTS; DISK;

D O I：

10.3847/1538-4357/ab3653

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present a chemical abundance analysis of four additional confirmed member stars of Tucana III, a Milky Way satellite galaxy candidate in the process of being tidally disrupted as it is accreted by the Galaxy. Two of these stars are centrally located in the core of the galaxy while the other two stars are located in the eastern and western tidal tails. The four stars have chemical abundance patterns consistent with the one previously studied star in Tucana III: they are moderately enhanced in r-process elements, i.e., they have <[Eu/Fe]> approximate to +0.4 dex. The non-neutron-capture elements generally follow trends seen in other dwarf galaxies, including a metallicity range of 0.44 dex and the expected trend in alpha-elements, i.e., the lower metallicity stars have higher Ca and Ti abundances. Overall, the chemical abundance patterns of these stars suggest that Tucana III was an ultra-faint dwarf galaxy, and not a globular cluster, before being tidally disturbed. As is the case for the one other galaxy dominated by r-process enhanced stars, Reticulum II, Tucana III's stellar chemical abundances are consistent with pollution from ejecta produced by a binary neutron star merger, although a different r-process element or dilution gas mass is required to explain the abundances in these two galaxies if a neutron star merger is the sole source of r-process enhancement.

引用

页数：12

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