The chemical characterization of halo substructure in the Milky Way based on APOGEE

被引：94

作者：

Horta, Danny ^{[1
,2
]}

Schiavon, Ricardo P. ^{[1
]}

Mackereth, J. Ted ^{[3
,4
]}

Weinberg, David H. ^{[5
]}

Hasselquist, Sten ^{[6
]}

Feuillet, Diane ^{[7
]}

O'Connell, Robert W. ^{[8
]}

Anguiano, Borja ^{[8
]}

Allende-Prieto, Carlos ^{[9
,10
]}

Beaton, Rachael L. ^{[11
]}

Bizyaev, Dmitry ^{[12
]}

Cunha, Katia ^{[13
,14
]}

Geisler, Doug ^{[15
,16
,17
]}

Garcia-Hernandez, D. A.

Holtzman, Jon

Joensson, Henrik ^{[18
]}

Lane, Richard R. ^{[19
]}

Majewski, Steve R.

Meszaros, Szabolcs ^{[20
,21
]}

Minniti, Dante ^{[22
,23
]}

Nitschelm, Christian ^{[24
]}

Shetrone, Matthew ^{[25
]}

Smith, Verne V. ^{[26
]}

Zasowski, Gail ^{[27
]}

机构：

[1] Astrophys Res Inst, 146 Brownlow Hill, Liverpool L35RF, England

[2] Univ Queensland, Sch Math & Phys, St Lucia, Qld 4072, Australia

[3] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada

[4] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S3H4, Canada

[5] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA

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

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

[8] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA

[9] Inst Astrofis Canarias IAC, E-38205 San Cristobal la Laguna, Tenerife, Spain

[10] Univ Laguna ULL, Dept Astrofis, E-38206 San Cristobal la Laguna, Tenerife, Spain

[11] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA

[12] New Mexico State Univ, Las Cruces, NM 88003 USA

[13] Univ Arizona, Tucson, AZ 85719 USA

[14] Observ Nacl, Sao Cristovao, RJ, Brazil

[15] Univ Concepcion, Dept Astron, Casilla 160-C, Concepcion, Chile

[16] Univ Serena, Inst Invest Multidisciplinario Ciencia & Tecnol, Ave Raul Bitran S-N, La Serena, Chile

[17] Univ Serena, Fac Ciencias, Dept Astron, Av Juan Cisternas 120, La Serena, Chile

[18] Malmo Univ, Mat Sci & Appl Math, SE-20506 Malmo, Sweden

[19] Univ Bernardo OHiggins, Ctr Invest Astron, Ave Viel 1497, Santiago, Chile

[20] Eotvos Lorand Univ, Gothard Astrophys Observ, SzentImreH st 112, H-9700 Szombathely, Hungary

[21] ELTE Lendulet Momentum Milky Way Res Grp, MTA, Szombathely, Hungary

[22] Univ Andres Bello, Fac Ciencias Exactas, Dept Ciencias Fis, Av Fernandez Concha 700, Santiago, Chile

[23] Vatican Observ, Vatican City V-00120, Vatican City St, Vatican

[24] Univ Antofagasta, Ctr Astron CITEVA, Ave Angamos 60, Antofagasta 1270300, Chile

[25] Univ Texas Austin, McDonald Observ, Austin, TX 79734 USA

[26] Natl Opt Astron Observ, Tucson, AZ 85719 USA

[27] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84105 USA

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2023年 / 520卷 / 04期

基金：

美国安德鲁·梅隆基金会;

关键词：

Galaxy: abundances; Galaxy: evolution; Galaxy: formation; Galaxy: general; Galaxy: halo; Galaxy: kinematics and dynamics; SAGITTARIUS DWARF GALAXY; DIGITAL SKY SURVEY; R-PROCESS ENRICHMENT; STELLAR HALO; GALACTIC HALO; SOLAR NEIGHBORHOOD; ABUNDANCE RATIOS; SURVEY VIEW; IN-SITU; ELEMENTAL ABUNDANCES;

D O I：

10.1093/mnras/stac3179

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Galactic haloes in a ?-CDM universe are predicted to host today a swarm of debris resulting from cannibalized dwarf galaxies. The chemodynamical information recorded in their stellar populations helps elucidate their nature, constraining the assembly history of the Galaxy. Using data from APOGEE and Gaia, we examine the chemical properties of various halo substructures, considering elements that sample various nucleosynthetic pathways. The systems studied are Heracles, Gaia-Enceladus/Sausage (GES), the Helmi stream, Sequoia, Thamnos, Aleph, LMS-1, Arjuna, I'itoi, Nyx, Icarus, and Pontus. Abundance patterns of all substructures are cross-compared in a statistically robust fashion. Our main findings include: (i) the chemical properties of most substructures studied match qualitatively those of dwarf Milky Way satellites, such as the Sagittarius dSph. Exceptions are Nyx and Aleph, which are chemically similar to disc stars, implying that these substructures were likely formed in situ; (ii) Heracles differs chemically from in situ populations such as Aurora and its inner halo counterparts in a statistically significant way. The differences suggest that the star formation rate was lower in Heracles than in the early Milky Way; (iii) the chemistry of Arjuna, LMS-1, and I'itoi is indistinguishable from that of GES, suggesting a possible common origin; (iv) all three Sequoia samples studied are qualitatively similar. However, only two of those samples present chemistry that is consistent with GES in a statistically significant fashion; (v) the abundance patterns of the Helmi stream and Thamnos are different from all other halo substructures.

引用

页码：5671 / 5711

页数：41

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