NAOC Open IR
Star Formation Timescales of the Halo Populations from Asteroseismology and Chemical Abundances*
Matsuno, Tadafumi1,2,3; Aoki, Wako2,3; Casagrande, Luca4; Ishigaki, Miho5; Shi, Jianrong6; Takata, Masao7; Xiang, Maosheng8; Yong, David4; Li, Haining6; Suda, Takuma9,10,11; Xing, Qianfan6; Zhao, Jingkun6
2021-05-01
Source PublicationASTROPHYSICAL JOURNAL
ISSN0004-637X
Volume912Issue:1Pages:38
AbstractWe combine asteroseismology, optical high-resolution spectroscopy, and kinematic analysis for 26 halo red giant branch stars in the Kepler field in the range of -2.5 < [Fe/H] < -0.6. After applying theoretically motivated corrections to the seismic scaling relations, we obtain an average mass of 0.97 +/- 0.03 M (circle dot) for our sample of halo stars. Although this maps into an age of similar to 7 Gyr, significantly younger than independent age estimates of the Milky Way stellar halo, we considered this apparently young age to be due to the overestimation of stellar mass in the scaling relations. There is no significant mass dispersion among lower red giant branch stars (log g > 2), which constrains the relative age dispersion to <18%, corresponding to -1.7 into two [Mg/Fe] groups. While the [alpha/Fe] and [Eu/Mg] ratios are different between the two subsamples, [s/Eu], where s stands for Ba, La, Ce, and Nd, does not show a significant difference. These abundance ratios suggest that the chemical evolution of the low-Mg population is contributed by Type Ia supernovae, but not by low- to intermediate-mass asymptotic giant branch stars, providing a constraint on its star formation timescale as 100 Myr < tau < 300 Myr. We also do not detect any significant mass difference between the two [Mg/Fe] groups, thus suggesting that their formation epochs are not separated by more than 1.5 Gyr.
KeywordHalo stars Asteroseismology Chemical abundances Stellar kinematics High resolution spectroscopy Stellar ages
Funding OrganizationJSPS-CAS Joint Research Program ; JSPS-CAS Joint Research Program ; course-by-course education program of SOKENDAI ; course-by-course education program of SOKENDAI ; JSPS KAKENHI ; JSPS KAKENHI ; Australian Research Council ; Australian Research Council ; NSFC ; NSFC ; Strategic Priority Research Program of the Chinese Academy of Sciences ; Strategic Priority Research Program of the Chinese Academy of Sciences ; JSPS-CAS Joint Research Program ; JSPS-CAS Joint Research Program ; course-by-course education program of SOKENDAI ; course-by-course education program of SOKENDAI ; JSPS KAKENHI ; JSPS KAKENHI ; Australian Research Council ; Australian Research Council ; NSFC ; NSFC ; Strategic Priority Research Program of the Chinese Academy of Sciences ; Strategic Priority Research Program of the Chinese Academy of Sciences ; JSPS-CAS Joint Research Program ; JSPS-CAS Joint Research Program ; course-by-course education program of SOKENDAI ; course-by-course education program of SOKENDAI ; JSPS KAKENHI ; JSPS KAKENHI ; Australian Research Council ; Australian Research Council ; NSFC ; NSFC ; Strategic Priority Research Program of the Chinese Academy of Sciences ; Strategic Priority Research Program of the Chinese Academy of Sciences ; JSPS-CAS Joint Research Program ; JSPS-CAS Joint Research Program ; course-by-course education program of SOKENDAI ; course-by-course education program of SOKENDAI ; JSPS KAKENHI ; JSPS KAKENHI ; Australian Research Council ; Australian Research Council ; NSFC ; NSFC ; Strategic Priority Research Program of the Chinese Academy of Sciences ; Strategic Priority Research Program of the Chinese Academy of Sciences
DOI10.3847/1538-4357/abeab2
Language英语
Funding ProjectJSPS-CAS Joint Research Program ; course-by-course education program of SOKENDAI ; JSPS KAKENHI[16H02168] ; JSPS KAKENHI[20HP8012] ; JSPS KAKENHI[16H02166] ; Australian Research Council[FT160100402] ; NSFC[11973049] ; Strategic Priority Research Program of the Chinese Academy of Sciences[XDB34020205] ; [18J11326]
Funding OrganizationJSPS-CAS Joint Research Program ; JSPS-CAS Joint Research Program ; course-by-course education program of SOKENDAI ; course-by-course education program of SOKENDAI ; JSPS KAKENHI ; JSPS KAKENHI ; Australian Research Council ; Australian Research Council ; NSFC ; NSFC ; Strategic Priority Research Program of the Chinese Academy of Sciences ; Strategic Priority Research Program of the Chinese Academy of Sciences ; JSPS-CAS Joint Research Program ; JSPS-CAS Joint Research Program ; course-by-course education program of SOKENDAI ; course-by-course education program of SOKENDAI ; JSPS KAKENHI ; JSPS KAKENHI ; Australian Research Council ; Australian Research Council ; NSFC ; NSFC ; Strategic Priority Research Program of the Chinese Academy of Sciences ; Strategic Priority Research Program of the Chinese Academy of Sciences ; JSPS-CAS Joint Research Program ; JSPS-CAS Joint Research Program ; course-by-course education program of SOKENDAI ; course-by-course education program of SOKENDAI ; JSPS KAKENHI ; JSPS KAKENHI ; Australian Research Council ; Australian Research Council ; NSFC ; NSFC ; Strategic Priority Research Program of the Chinese Academy of Sciences ; Strategic Priority Research Program of the Chinese Academy of Sciences ; JSPS-CAS Joint Research Program ; JSPS-CAS Joint Research Program ; course-by-course education program of SOKENDAI ; course-by-course education program of SOKENDAI ; JSPS KAKENHI ; JSPS KAKENHI ; Australian Research Council ; Australian Research Council ; NSFC ; NSFC ; Strategic Priority Research Program of the Chinese Academy of Sciences ; Strategic Priority Research Program of the Chinese Academy of Sciences
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS IDWOS:000648778400001
PublisherIOP PUBLISHING LTD
Citation statistics
Document Type期刊论文
Identifierhttp://ir.bao.ac.cn/handle/114a11/78109
Collection中国科学院国家天文台
Corresponding AuthorMatsuno, Tadafumi
Affiliation1.Univ Groningen, Kapteyn Astron Inst, Landleven 12, NL-9747 AD Groningen, Netherlands
2.SOKENDAI, Sch Phys Sci, Dept Astron Sci, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan
3.Natl Astron Observ Japan NAOJ, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan
4.Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2611, Australia
5.Tohoku Univ, Astron Inst, Sendai, Miyagi 9808578, Japan
6.Chinese Acad Sci, Natl Astron Observ, Key Lab Opt Astron, Beijing 100101, Peoples R China
7.Univ Tokyo, Sch Sci, Dept Astron, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan
8.Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany
9.Open Univ Japan, Mihama Ku, Wakaba 2-11, Chiba 2618586, Japan
10.Univ Tokyo, Res Ctr Early Universe, Bunkyo Ku, Hongo 7-3-1, Tokyo 1130033, Japan
11.Tokyo Univ Technol, Dept Liberal Arts, Ota Ku, Nishi Kamata 5-23-22, Tokyo 1448535, Japan
Recommended Citation
GB/T 7714
Matsuno, Tadafumi,Aoki, Wako,Casagrande, Luca,et al. Star Formation Timescales of the Halo Populations from Asteroseismology and Chemical Abundances*[J]. ASTROPHYSICAL JOURNAL,2021,912(1):38.
APA Matsuno, Tadafumi.,Aoki, Wako.,Casagrande, Luca.,Ishigaki, Miho.,Shi, Jianrong.,...&Zhao, Jingkun.(2021).Star Formation Timescales of the Halo Populations from Asteroseismology and Chemical Abundances*.ASTROPHYSICAL JOURNAL,912(1),38.
MLA Matsuno, Tadafumi,et al."Star Formation Timescales of the Halo Populations from Asteroseismology and Chemical Abundances*".ASTROPHYSICAL JOURNAL 912.1(2021):38.
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