Search for Extremely Metal-poor Stars with Gemini-N/Graces. I. Chemical-abundance Analysis

We present stellar parameters and abundances of 13 elements for 18 very metal-poor (VMP; [Fe/H] < –2.0) stars, selected as extremely metal-poor (EMP; [Fe/H] < –3.0) candidates from the Sloan Digital Sky Survey and Large sky Area Multi-Object Fiber Spectroscopic Telescope survey. High-resolutio...
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Autor*in:	Miji Jeong [verfasserIn] Young Sun Lee [verfasserIn] Timothy C. Beers [verfasserIn] Vinicius M. Placco [verfasserIn] Young Kwang Kim [verfasserIn] Jae-Rim Koo [verfasserIn] Ho-Gyu Lee [verfasserIn] Soung-Chul Yang [verfasserIn]

Format:	E-Artikel
Sprache:	Englisch

Erschienen:	2023

Schlagwörter:	Chemical abundances Galaxy chemical evolution Milky Way Galaxy Interstellar abundances Galaxy stellar content

Übergeordnetes Werk:	In: The Astrophysical Journal - IOP Publishing, 2022, 948(2023), 1, p 38
Übergeordnetes Werk:	volume:948 ; year:2023 ; number:1, p 38

Links:	Link aufrufen Link aufrufen Link aufrufen Journal toc

DOI / URN:	10.3847/1538-4357/acc58a

Katalog-ID:	DOAJ090134273

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520			\|a We present stellar parameters and abundances of 13 elements for 18 very metal-poor (VMP; [Fe/H] < –2.0) stars, selected as extremely metal-poor (EMP; [Fe/H] < –3.0) candidates from the Sloan Digital Sky Survey and Large sky Area Multi-Object Fiber Spectroscopic Telescope survey. High-resolution spectroscopic observations were performed using GEMINI-N/GRACES. We find 10 EMP stars among our candidates, and we newly identify three carbon-enhanced metal-poor stars with [Ba/Fe] < 0. Although chemical abundances of our VMP/EMP stars generally follow the overall trend of other Galactic halo stars, there are a few exceptions. One Na-rich star ([Na/Fe] = +1.14) with low [Mg/Fe] suggests a possible chemical connection with second-generation stars in a globular cluster. The progenitor of an extremely Na-poor star ([Na/Fe] = –1.02) with high K- and Ni-abundance ratios may have undergone a distinct nucleosynthesis episode, associated with core-collapse supernovae (SNe) having a high explosion energy. We have also found a Mg-rich star ([Mg/Fe] = +0.73) with slightly enhanced Na and extremely low [Ba/Fe], indicating that its origin is not associated with neutron-capture events. On the other hand, the origin of the lowest Mg abundance ([Mg/Fe] = –0.61) star could be explained by accretion from a dwarf galaxy, or formation in a gas cloud largely polluted by SNe Ia. We have also explored the progenitor masses of our EMP stars by comparing their chemical-abundance patterns with those predicted by Population III SNe models, and find a mass range of 10–26 M _⊙ , suggesting that such stars were primarily responsible for the chemical enrichment of the early Milky Way.
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allfields	10.3847/1538-4357/acc58a doi (DE-627)DOAJ090134273 (DE-599)DOAJcf7c41e88e7b4ba38de38fdf18a4ce10 DE-627 ger DE-627 rakwb eng QB460-466 Miji Jeong verfasserin aut Search for Extremely Metal-poor Stars with Gemini-N/Graces. I. Chemical-abundance Analysis 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We present stellar parameters and abundances of 13 elements for 18 very metal-poor (VMP; [Fe/H] < –2.0) stars, selected as extremely metal-poor (EMP; [Fe/H] < –3.0) candidates from the Sloan Digital Sky Survey and Large sky Area Multi-Object Fiber Spectroscopic Telescope survey. High-resolution spectroscopic observations were performed using GEMINI-N/GRACES. We find 10 EMP stars among our candidates, and we newly identify three carbon-enhanced metal-poor stars with [Ba/Fe] < 0. Although chemical abundances of our VMP/EMP stars generally follow the overall trend of other Galactic halo stars, there are a few exceptions. One Na-rich star ([Na/Fe] = +1.14) with low [Mg/Fe] suggests a possible chemical connection with second-generation stars in a globular cluster. The progenitor of an extremely Na-poor star ([Na/Fe] = –1.02) with high K- and Ni-abundance ratios may have undergone a distinct nucleosynthesis episode, associated with core-collapse supernovae (SNe) having a high explosion energy. We have also found a Mg-rich star ([Mg/Fe] = +0.73) with slightly enhanced Na and extremely low [Ba/Fe], indicating that its origin is not associated with neutron-capture events. On the other hand, the origin of the lowest Mg abundance ([Mg/Fe] = –0.61) star could be explained by accretion from a dwarf galaxy, or formation in a gas cloud largely polluted by SNe Ia. We have also explored the progenitor masses of our EMP stars by comparing their chemical-abundance patterns with those predicted by Population III SNe models, and find a mass range of 10–26 M _⊙ , suggesting that such stars were primarily responsible for the chemical enrichment of the early Milky Way. Chemical abundances Galaxy chemical evolution Milky Way Galaxy Interstellar abundances Galaxy stellar content Astrophysics Young Sun Lee verfasserin aut Timothy C. Beers verfasserin aut Vinicius M. Placco verfasserin aut Young Kwang Kim verfasserin aut Jae-Rim Koo verfasserin aut Ho-Gyu Lee verfasserin aut Soung-Chul Yang verfasserin aut In The Astrophysical Journal IOP Publishing, 2022 948(2023), 1, p 38 (DE-627)269019219 (DE-600)1473835-1 15384357 nnns volume:948 year:2023 number:1, p 38 https://doi.org/10.3847/1538-4357/acc58a kostenfrei https://doaj.org/article/cf7c41e88e7b4ba38de38fdf18a4ce10 kostenfrei https://doi.org/10.3847/1538-4357/acc58a kostenfrei https://doaj.org/toc/1538-4357 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 948 2023 1, p 38
spelling	10.3847/1538-4357/acc58a doi (DE-627)DOAJ090134273 (DE-599)DOAJcf7c41e88e7b4ba38de38fdf18a4ce10 DE-627 ger DE-627 rakwb eng QB460-466 Miji Jeong verfasserin aut Search for Extremely Metal-poor Stars with Gemini-N/Graces. I. Chemical-abundance Analysis 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We present stellar parameters and abundances of 13 elements for 18 very metal-poor (VMP; [Fe/H] < –2.0) stars, selected as extremely metal-poor (EMP; [Fe/H] < –3.0) candidates from the Sloan Digital Sky Survey and Large sky Area Multi-Object Fiber Spectroscopic Telescope survey. High-resolution spectroscopic observations were performed using GEMINI-N/GRACES. We find 10 EMP stars among our candidates, and we newly identify three carbon-enhanced metal-poor stars with [Ba/Fe] < 0. Although chemical abundances of our VMP/EMP stars generally follow the overall trend of other Galactic halo stars, there are a few exceptions. One Na-rich star ([Na/Fe] = +1.14) with low [Mg/Fe] suggests a possible chemical connection with second-generation stars in a globular cluster. The progenitor of an extremely Na-poor star ([Na/Fe] = –1.02) with high K- and Ni-abundance ratios may have undergone a distinct nucleosynthesis episode, associated with core-collapse supernovae (SNe) having a high explosion energy. We have also found a Mg-rich star ([Mg/Fe] = +0.73) with slightly enhanced Na and extremely low [Ba/Fe], indicating that its origin is not associated with neutron-capture events. On the other hand, the origin of the lowest Mg abundance ([Mg/Fe] = –0.61) star could be explained by accretion from a dwarf galaxy, or formation in a gas cloud largely polluted by SNe Ia. We have also explored the progenitor masses of our EMP stars by comparing their chemical-abundance patterns with those predicted by Population III SNe models, and find a mass range of 10–26 M _⊙ , suggesting that such stars were primarily responsible for the chemical enrichment of the early Milky Way. Chemical abundances Galaxy chemical evolution Milky Way Galaxy Interstellar abundances Galaxy stellar content Astrophysics Young Sun Lee verfasserin aut Timothy C. Beers verfasserin aut Vinicius M. Placco verfasserin aut Young Kwang Kim verfasserin aut Jae-Rim Koo verfasserin aut Ho-Gyu Lee verfasserin aut Soung-Chul Yang verfasserin aut In The Astrophysical Journal IOP Publishing, 2022 948(2023), 1, p 38 (DE-627)269019219 (DE-600)1473835-1 15384357 nnns volume:948 year:2023 number:1, p 38 https://doi.org/10.3847/1538-4357/acc58a kostenfrei https://doaj.org/article/cf7c41e88e7b4ba38de38fdf18a4ce10 kostenfrei https://doi.org/10.3847/1538-4357/acc58a kostenfrei https://doaj.org/toc/1538-4357 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 948 2023 1, p 38
allfields_unstemmed	10.3847/1538-4357/acc58a doi (DE-627)DOAJ090134273 (DE-599)DOAJcf7c41e88e7b4ba38de38fdf18a4ce10 DE-627 ger DE-627 rakwb eng QB460-466 Miji Jeong verfasserin aut Search for Extremely Metal-poor Stars with Gemini-N/Graces. I. Chemical-abundance Analysis 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We present stellar parameters and abundances of 13 elements for 18 very metal-poor (VMP; [Fe/H] < –2.0) stars, selected as extremely metal-poor (EMP; [Fe/H] < –3.0) candidates from the Sloan Digital Sky Survey and Large sky Area Multi-Object Fiber Spectroscopic Telescope survey. High-resolution spectroscopic observations were performed using GEMINI-N/GRACES. We find 10 EMP stars among our candidates, and we newly identify three carbon-enhanced metal-poor stars with [Ba/Fe] < 0. Although chemical abundances of our VMP/EMP stars generally follow the overall trend of other Galactic halo stars, there are a few exceptions. One Na-rich star ([Na/Fe] = +1.14) with low [Mg/Fe] suggests a possible chemical connection with second-generation stars in a globular cluster. The progenitor of an extremely Na-poor star ([Na/Fe] = –1.02) with high K- and Ni-abundance ratios may have undergone a distinct nucleosynthesis episode, associated with core-collapse supernovae (SNe) having a high explosion energy. We have also found a Mg-rich star ([Mg/Fe] = +0.73) with slightly enhanced Na and extremely low [Ba/Fe], indicating that its origin is not associated with neutron-capture events. On the other hand, the origin of the lowest Mg abundance ([Mg/Fe] = –0.61) star could be explained by accretion from a dwarf galaxy, or formation in a gas cloud largely polluted by SNe Ia. We have also explored the progenitor masses of our EMP stars by comparing their chemical-abundance patterns with those predicted by Population III SNe models, and find a mass range of 10–26 M _⊙ , suggesting that such stars were primarily responsible for the chemical enrichment of the early Milky Way. Chemical abundances Galaxy chemical evolution Milky Way Galaxy Interstellar abundances Galaxy stellar content Astrophysics Young Sun Lee verfasserin aut Timothy C. Beers verfasserin aut Vinicius M. Placco verfasserin aut Young Kwang Kim verfasserin aut Jae-Rim Koo verfasserin aut Ho-Gyu Lee verfasserin aut Soung-Chul Yang verfasserin aut In The Astrophysical Journal IOP Publishing, 2022 948(2023), 1, p 38 (DE-627)269019219 (DE-600)1473835-1 15384357 nnns volume:948 year:2023 number:1, p 38 https://doi.org/10.3847/1538-4357/acc58a kostenfrei https://doaj.org/article/cf7c41e88e7b4ba38de38fdf18a4ce10 kostenfrei https://doi.org/10.3847/1538-4357/acc58a kostenfrei https://doaj.org/toc/1538-4357 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 948 2023 1, p 38
allfieldsGer	10.3847/1538-4357/acc58a doi (DE-627)DOAJ090134273 (DE-599)DOAJcf7c41e88e7b4ba38de38fdf18a4ce10 DE-627 ger DE-627 rakwb eng QB460-466 Miji Jeong verfasserin aut Search for Extremely Metal-poor Stars with Gemini-N/Graces. I. Chemical-abundance Analysis 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We present stellar parameters and abundances of 13 elements for 18 very metal-poor (VMP; [Fe/H] < –2.0) stars, selected as extremely metal-poor (EMP; [Fe/H] < –3.0) candidates from the Sloan Digital Sky Survey and Large sky Area Multi-Object Fiber Spectroscopic Telescope survey. High-resolution spectroscopic observations were performed using GEMINI-N/GRACES. We find 10 EMP stars among our candidates, and we newly identify three carbon-enhanced metal-poor stars with [Ba/Fe] < 0. Although chemical abundances of our VMP/EMP stars generally follow the overall trend of other Galactic halo stars, there are a few exceptions. One Na-rich star ([Na/Fe] = +1.14) with low [Mg/Fe] suggests a possible chemical connection with second-generation stars in a globular cluster. The progenitor of an extremely Na-poor star ([Na/Fe] = –1.02) with high K- and Ni-abundance ratios may have undergone a distinct nucleosynthesis episode, associated with core-collapse supernovae (SNe) having a high explosion energy. We have also found a Mg-rich star ([Mg/Fe] = +0.73) with slightly enhanced Na and extremely low [Ba/Fe], indicating that its origin is not associated with neutron-capture events. On the other hand, the origin of the lowest Mg abundance ([Mg/Fe] = –0.61) star could be explained by accretion from a dwarf galaxy, or formation in a gas cloud largely polluted by SNe Ia. We have also explored the progenitor masses of our EMP stars by comparing their chemical-abundance patterns with those predicted by Population III SNe models, and find a mass range of 10–26 M _⊙ , suggesting that such stars were primarily responsible for the chemical enrichment of the early Milky Way. Chemical abundances Galaxy chemical evolution Milky Way Galaxy Interstellar abundances Galaxy stellar content Astrophysics Young Sun Lee verfasserin aut Timothy C. Beers verfasserin aut Vinicius M. Placco verfasserin aut Young Kwang Kim verfasserin aut Jae-Rim Koo verfasserin aut Ho-Gyu Lee verfasserin aut Soung-Chul Yang verfasserin aut In The Astrophysical Journal IOP Publishing, 2022 948(2023), 1, p 38 (DE-627)269019219 (DE-600)1473835-1 15384357 nnns volume:948 year:2023 number:1, p 38 https://doi.org/10.3847/1538-4357/acc58a kostenfrei https://doaj.org/article/cf7c41e88e7b4ba38de38fdf18a4ce10 kostenfrei https://doi.org/10.3847/1538-4357/acc58a kostenfrei https://doaj.org/toc/1538-4357 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 948 2023 1, p 38
allfieldsSound	10.3847/1538-4357/acc58a doi (DE-627)DOAJ090134273 (DE-599)DOAJcf7c41e88e7b4ba38de38fdf18a4ce10 DE-627 ger DE-627 rakwb eng QB460-466 Miji Jeong verfasserin aut Search for Extremely Metal-poor Stars with Gemini-N/Graces. I. Chemical-abundance Analysis 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We present stellar parameters and abundances of 13 elements for 18 very metal-poor (VMP; [Fe/H] < –2.0) stars, selected as extremely metal-poor (EMP; [Fe/H] < –3.0) candidates from the Sloan Digital Sky Survey and Large sky Area Multi-Object Fiber Spectroscopic Telescope survey. High-resolution spectroscopic observations were performed using GEMINI-N/GRACES. We find 10 EMP stars among our candidates, and we newly identify three carbon-enhanced metal-poor stars with [Ba/Fe] < 0. Although chemical abundances of our VMP/EMP stars generally follow the overall trend of other Galactic halo stars, there are a few exceptions. One Na-rich star ([Na/Fe] = +1.14) with low [Mg/Fe] suggests a possible chemical connection with second-generation stars in a globular cluster. The progenitor of an extremely Na-poor star ([Na/Fe] = –1.02) with high K- and Ni-abundance ratios may have undergone a distinct nucleosynthesis episode, associated with core-collapse supernovae (SNe) having a high explosion energy. We have also found a Mg-rich star ([Mg/Fe] = +0.73) with slightly enhanced Na and extremely low [Ba/Fe], indicating that its origin is not associated with neutron-capture events. On the other hand, the origin of the lowest Mg abundance ([Mg/Fe] = –0.61) star could be explained by accretion from a dwarf galaxy, or formation in a gas cloud largely polluted by SNe Ia. We have also explored the progenitor masses of our EMP stars by comparing their chemical-abundance patterns with those predicted by Population III SNe models, and find a mass range of 10–26 M _⊙ , suggesting that such stars were primarily responsible for the chemical enrichment of the early Milky Way. Chemical abundances Galaxy chemical evolution Milky Way Galaxy Interstellar abundances Galaxy stellar content Astrophysics Young Sun Lee verfasserin aut Timothy C. Beers verfasserin aut Vinicius M. Placco verfasserin aut Young Kwang Kim verfasserin aut Jae-Rim Koo verfasserin aut Ho-Gyu Lee verfasserin aut Soung-Chul Yang verfasserin aut In The Astrophysical Journal IOP Publishing, 2022 948(2023), 1, p 38 (DE-627)269019219 (DE-600)1473835-1 15384357 nnns volume:948 year:2023 number:1, p 38 https://doi.org/10.3847/1538-4357/acc58a kostenfrei https://doaj.org/article/cf7c41e88e7b4ba38de38fdf18a4ce10 kostenfrei https://doi.org/10.3847/1538-4357/acc58a kostenfrei https://doaj.org/toc/1538-4357 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 948 2023 1, p 38
language	English
source	In The Astrophysical Journal 948(2023), 1, p 38 volume:948 year:2023 number:1, p 38
sourceStr	In The Astrophysical Journal 948(2023), 1, p 38 volume:948 year:2023 number:1, p 38
format_phy_str_mv	Article
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topic_facet	Chemical abundances Galaxy chemical evolution Milky Way Galaxy Interstellar abundances Galaxy stellar content Astrophysics
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container_title	The Astrophysical Journal
authorswithroles_txt_mv	Miji Jeong @@aut@@ Young Sun Lee @@aut@@ Timothy C. Beers @@aut@@ Vinicius M. Placco @@aut@@ Young Kwang Kim @@aut@@ Jae-Rim Koo @@aut@@ Ho-Gyu Lee @@aut@@ Soung-Chul Yang @@aut@@
publishDateDaySort_date	2023-01-01T00:00:00Z
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topic_title	QB460-466 Search for Extremely Metal-poor Stars with Gemini-N/Graces. I. Chemical-abundance Analysis Chemical abundances Galaxy chemical evolution Milky Way Galaxy Interstellar abundances Galaxy stellar content
topic	misc QB460-466 misc Chemical abundances misc Galaxy chemical evolution misc Milky Way Galaxy misc Interstellar abundances misc Galaxy stellar content misc Astrophysics
topic_unstemmed	misc QB460-466 misc Chemical abundances misc Galaxy chemical evolution misc Milky Way Galaxy misc Interstellar abundances misc Galaxy stellar content misc Astrophysics
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title	Search for Extremely Metal-poor Stars with Gemini-N/Graces. I. Chemical-abundance Analysis
ctrlnum	(DE-627)DOAJ090134273 (DE-599)DOAJcf7c41e88e7b4ba38de38fdf18a4ce10
title_full	Search for Extremely Metal-poor Stars with Gemini-N/Graces. I. Chemical-abundance Analysis
author_sort	Miji Jeong
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author_browse	Miji Jeong Young Sun Lee Timothy C. Beers Vinicius M. Placco Young Kwang Kim Jae-Rim Koo Ho-Gyu Lee Soung-Chul Yang
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title_sort	search for extremely metal-poor stars with gemini-n/graces. i. chemical-abundance analysis
callnumber	QB460-466
title_auth	Search for Extremely Metal-poor Stars with Gemini-N/Graces. I. Chemical-abundance Analysis
abstract	We present stellar parameters and abundances of 13 elements for 18 very metal-poor (VMP; [Fe/H] < –2.0) stars, selected as extremely metal-poor (EMP; [Fe/H] < –3.0) candidates from the Sloan Digital Sky Survey and Large sky Area Multi-Object Fiber Spectroscopic Telescope survey. High-resolution spectroscopic observations were performed using GEMINI-N/GRACES. We find 10 EMP stars among our candidates, and we newly identify three carbon-enhanced metal-poor stars with [Ba/Fe] < 0. Although chemical abundances of our VMP/EMP stars generally follow the overall trend of other Galactic halo stars, there are a few exceptions. One Na-rich star ([Na/Fe] = +1.14) with low [Mg/Fe] suggests a possible chemical connection with second-generation stars in a globular cluster. The progenitor of an extremely Na-poor star ([Na/Fe] = –1.02) with high K- and Ni-abundance ratios may have undergone a distinct nucleosynthesis episode, associated with core-collapse supernovae (SNe) having a high explosion energy. We have also found a Mg-rich star ([Mg/Fe] = +0.73) with slightly enhanced Na and extremely low [Ba/Fe], indicating that its origin is not associated with neutron-capture events. On the other hand, the origin of the lowest Mg abundance ([Mg/Fe] = –0.61) star could be explained by accretion from a dwarf galaxy, or formation in a gas cloud largely polluted by SNe Ia. We have also explored the progenitor masses of our EMP stars by comparing their chemical-abundance patterns with those predicted by Population III SNe models, and find a mass range of 10–26 M _⊙ , suggesting that such stars were primarily responsible for the chemical enrichment of the early Milky Way.
abstractGer	We present stellar parameters and abundances of 13 elements for 18 very metal-poor (VMP; [Fe/H] < –2.0) stars, selected as extremely metal-poor (EMP; [Fe/H] < –3.0) candidates from the Sloan Digital Sky Survey and Large sky Area Multi-Object Fiber Spectroscopic Telescope survey. High-resolution spectroscopic observations were performed using GEMINI-N/GRACES. We find 10 EMP stars among our candidates, and we newly identify three carbon-enhanced metal-poor stars with [Ba/Fe] < 0. Although chemical abundances of our VMP/EMP stars generally follow the overall trend of other Galactic halo stars, there are a few exceptions. One Na-rich star ([Na/Fe] = +1.14) with low [Mg/Fe] suggests a possible chemical connection with second-generation stars in a globular cluster. The progenitor of an extremely Na-poor star ([Na/Fe] = –1.02) with high K- and Ni-abundance ratios may have undergone a distinct nucleosynthesis episode, associated with core-collapse supernovae (SNe) having a high explosion energy. We have also found a Mg-rich star ([Mg/Fe] = +0.73) with slightly enhanced Na and extremely low [Ba/Fe], indicating that its origin is not associated with neutron-capture events. On the other hand, the origin of the lowest Mg abundance ([Mg/Fe] = –0.61) star could be explained by accretion from a dwarf galaxy, or formation in a gas cloud largely polluted by SNe Ia. We have also explored the progenitor masses of our EMP stars by comparing their chemical-abundance patterns with those predicted by Population III SNe models, and find a mass range of 10–26 M _⊙ , suggesting that such stars were primarily responsible for the chemical enrichment of the early Milky Way.
abstract_unstemmed	We present stellar parameters and abundances of 13 elements for 18 very metal-poor (VMP; [Fe/H] < –2.0) stars, selected as extremely metal-poor (EMP; [Fe/H] < –3.0) candidates from the Sloan Digital Sky Survey and Large sky Area Multi-Object Fiber Spectroscopic Telescope survey. High-resolution spectroscopic observations were performed using GEMINI-N/GRACES. We find 10 EMP stars among our candidates, and we newly identify three carbon-enhanced metal-poor stars with [Ba/Fe] < 0. Although chemical abundances of our VMP/EMP stars generally follow the overall trend of other Galactic halo stars, there are a few exceptions. One Na-rich star ([Na/Fe] = +1.14) with low [Mg/Fe] suggests a possible chemical connection with second-generation stars in a globular cluster. The progenitor of an extremely Na-poor star ([Na/Fe] = –1.02) with high K- and Ni-abundance ratios may have undergone a distinct nucleosynthesis episode, associated with core-collapse supernovae (SNe) having a high explosion energy. We have also found a Mg-rich star ([Mg/Fe] = +0.73) with slightly enhanced Na and extremely low [Ba/Fe], indicating that its origin is not associated with neutron-capture events. On the other hand, the origin of the lowest Mg abundance ([Mg/Fe] = –0.61) star could be explained by accretion from a dwarf galaxy, or formation in a gas cloud largely polluted by SNe Ia. We have also explored the progenitor masses of our EMP stars by comparing their chemical-abundance patterns with those predicted by Population III SNe models, and find a mass range of 10–26 M _⊙ , suggesting that such stars were primarily responsible for the chemical enrichment of the early Milky Way.
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container_issue	1, p 38
title_short	Search for Extremely Metal-poor Stars with Gemini-N/Graces. I. Chemical-abundance Analysis
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