Chemical Analysis of the Brightest Star of the Cetus II Ultrafaint Dwarf Galaxy Candidate

被引：2

作者：

Webber, K. B. ^{[1
,2
]}

Hansen, T. T. ^{[3
]}

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

Simon, J. D. ^{[4
]}

Pace, A. B. ^{[5
]}

Mutlu-Pakdil, B. ^{[6
]}

Drlica-Wagner, A. ^{[7
,8
,9
]}

Martinez-Vazquez, C. E. ^{[10
,11
]}

Aguena, M. ^{[12
]}

Allam, S. S. ^{[7
]}

Alves, O. ^{[13
]}

Bertin, E. ^{[14
,15
]}

Brooks, D. ^{[16
]}

Carnero Rosell, A. ^{[12
,17
,18
]}

Carretero, J. ^{[19
]}

da Costa, L. N. ^{[12
]}

De Vicente, J. ^{[20
]}

Doel, P. ^{[16
]}

Ferrero, I. ^{[21
]}

Friedel, D. ^{[22
]}

Frieman, J. ^{[7
,8
]}

Garcia-Bellido, J. ^{[23
]}

Giannini, G. ^{[19
]}

Gruen, D. ^{[24
]}

Gruendl, R. A. ^{[22
,25
]}

Hinton, S. R. ^{[26
]}

Hollowood, D. L. ^{[27
]}

Honscheid, K. ^{[28
,29
]}

Kuehn, K. ^{[30
,31
]}

Mena-Fernandez, J. ^{[20
]}

Menanteau, F. ^{[22
,25
]}

Miquel, R. ^{[19
,32
]}

Ogando, R. L. C. ^{[33
]}

Pereira, M. E. S. ^{[34
]}

Pieres, A. ^{[12
,33
]}

Plazas Malagon, A. A. ^{[35
,36
]}

Sanchez, E. ^{[20
]}

Santiago, B. ^{[12
,37
]}

Smith, J. Allyn ^{[38
]}

Smith, M. ^{[39
]}

Suchyta, E. ^{[40
]}

Tarle, G. ^{[13
]}

To, C. ^{[28
]}

Weaverdyck, N. ^{[13
,41
]}

Yanny, B. ^{[7
]}

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] Stockholm Univ, Dept Astron, AlbaNova Univ Ctr, SE-10691 Stockholm, Sweden

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

[5] Carnegie Mellon Univ, McWilliams Ctr Cosmol, 5000 Forbes Ave, Pittsburgh, PA 15213 USA

[6] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA

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

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

[9] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA

[10] NSFs NOIRLab, Gemini Observ, 670 N Aohoku Pl, Hilo, HI 96720 USA

[11] NSFs NOIRLab, Cerro Tololo Interamer Observ, Casilla 603, La Serena, Chile

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

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

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

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

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

[17] Inst Astrofis Canarias, E-38205 Tenerife, Spain

[18] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain

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

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

[21] Univ Oslo, Inst Theoret Astrophys, POB 1029 Blindern, NO-0315 Oslo, Norway

[22] Natl Ctr Supercomp Applicat, Ctr Astrophys Surveys, 1205 West Clark St, Urbana, IL 61801 USA

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

[24] Ludwig Maximilians Univ Munchen, Univ Observ, Fac Phys, Scheinerstr 1, D-81679 Munich, Germany

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

[26] Univ Queensland, Sch Math & Phys, Brisbane, Qld 4072, Australia

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

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

[29] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA

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

[31] Lowell Observ, 1400 Mars Hill Rd, Flagstaff, AZ 86001 USA

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

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

[34] Univ Hamburg, Hamburger Sternwarte, Gojenbergsweg 112, D-21029 Hamburg, Germany

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

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

[37] UFRGS, Inst Fis, Caixa Postal 15051, BR-91501970 Rio De Janeiro, RJ, Brazil

[38] Austin Peay State Univ, Dept Phys Engn & Astron, POB 4608, Clarksville, TN 37044 USA

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

[40] Oak Ridge Natl Lab, Comp Sci & Math Div, Oak Ridge, TN 37831 USA

[41] Lawrence Berkeley Natl Lab, 1 Cyclotron Rd, Berkeley, CA 94720 USA

来源：

ASTROPHYSICAL JOURNAL | 2023年 / 959卷 / 02期

基金：

美国国家科学基金会;

关键词：

METAL-POOR STARS; HIGH-RESOLUTION SPECTROSCOPY; NEUTRON-CAPTURE ELEMENTS; PROCESS ENHANCED STAR; MILKY-WAY SATELLITES; NON-LTE ANALYSIS; ABUNDANCE DETERMINATIONS; LOG(GF) VALUES; GLOBULAR-CLUSTER; OSCILLATOR-STRENGTHS;

D O I：

10.3847/1538-4357/ad0385

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present a detailed chemical abundance analysis of the brightest star in the ultrafaint dwarf (UFD) galaxy candidate Cetus II from high-resolution Magellan/MIKE spectra. For this star, DES J011740.53-173053, abundances or upper limits of 18 elements from carbon to europium are derived. Its chemical abundances generally follow those of other UFD galaxy stars, with a slight enhancement of the alpha-elements (Mg, Si, and Ca) and low neutron-capture element (Sr, Ba, and Eu) abundances supporting the classification of Cetus II as a likely UFD. The star exhibits lower Sc, Ti, and V abundances than Milky Way (MW) halo stars with similar metallicity. This signature is consistent with yields from a supernova originating from a star with a mass of similar to 11.2 M-circle dot. In addition, the star has a potassium abundance of [K/Fe] = 0.81, which is somewhat higher than the K abundances of MW halo stars with similar metallicity, a signature that is also present in a number of UFD galaxies. A comparison including globular clusters and stellar stream stars suggests that high K is a specific characteristic of some UFD galaxy stars and can thus be used to help classify objects as UFD galaxies.

引用

页数：11

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