Raising the observed metallicity floor with a 3D non-LTE analysis of SDSS J102915.14+172927.9
Context: The first stars produced the first heavy elements and set the stage for the formation of the first galaxies. Accurate chemical abundances of ultra metal-poor stars ([Fe/H]
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| creator | Lagae, C Amarsi, A M Rodríguez Díaz, L F Lind, K Nordlander, T Hansen, T T Heger, A |
| description | Context: The first stars produced the first heavy elements and set the stage for the formation of the first galaxies. Accurate chemical abundances of ultra metal-poor stars ([Fe/H] |
| doi_str_mv | 10.48550/arxiv.2303.01374 |
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Accurate chemical abundances of ultra metal-poor stars ([Fe/H]<-4) can be used to infer properties of the first stars, and thus the formation mechanism for low-mass second generation stars in the early universe. Spectroscopic studies have shown that most second generation stars are carbon-enhanced with one notable exception SDSS J102915.14+172927.9. Aims: We reanalyse the composition of SDSS J102915.14+172927.9. Methods: We developed a tailored 3D model atmosphere for SDSS J102915.14+172927.9 with the Stagger-code, making use of an improved surface gravity estimate based on the Gaia DR3 parallax. This model was used as input in the radiative transfer code Balder to compute 3D non-LTE synthetic spectra. These spectra were then used to infer abundances for Mg, Si, Ca, Fe and Ni, and upper limits on Li, Na and Al. 3D LTE synthetic spectra were computed with Scate to infer the abundance of Ti and upper limits on C and N. Results: In contrast to earlier works based on 1D non-LTE corrections to 3D LTE results, we are able to achieve ionisation balance for Ca I and Ca II when employing our consistent 3D non-LTE treatment. Moreover, the elemental abundances are systematically higher than those found in earlier works. In particular, [Fe/H] increases by 0.57 dex, and the upper limits of C and N increase by 0.90 dex and 1.82 dex, respectively. Conclusions: We find that Population III progenitors with masses 10-20 M_sun exploding with energy E<=3*10^{51} erg can reproduce our 3D non-LTE abundance pattern. Contrary to previous work, we obtain higher upper limits on the carbon abundance that are ``marginally consistent'' with star formation through atomic line cooling, and as such, prevent strong conclusions about the formation mechanism of this low mass star.</description><identifier>EISSN: 2331-8422</identifier><identifier>DOI: 10.48550/arxiv.2303.01374</identifier><language>eng</language><publisher>Ithaca: Cornell University Library, arXiv.org</publisher><subject>Abundance ; Calcium ; Carbon ; Galaxies ; Heavy elements ; Iron ; Low mass stars ; Metallicity ; Parallax ; Physics - Astrophysics of Galaxies ; Physics - Solar and Stellar Astrophysics ; Radiative transfer ; Spectra ; Star & galaxy formation ; Star formation ; Three dimensional models ; Titanium</subject><ispartof>arXiv.org, 2023-03</ispartof><rights>2023. This work is published under http://creativecommons.org/licenses/by/4.0/ (the “License”). Notwithstanding the ProQuest Terms and Conditions, you may use this content in accordance with the terms of the License.</rights><rights>http://creativecommons.org/licenses/by/4.0</rights><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>228,230,780,784,885,27923</link.rule.ids><backlink>$$Uhttps://doi.org/10.48550/arXiv.2303.01374$$DView paper in arXiv$$Hfree_for_read</backlink><backlink>$$Uhttps://doi.org/10.1051/0004-6361/202245786$$DView published paper (Access to full text may be restricted)$$Hfree_for_read</backlink></links><search><creatorcontrib>Lagae, C</creatorcontrib><creatorcontrib>Amarsi, A M</creatorcontrib><creatorcontrib>Rodríguez Díaz, L F</creatorcontrib><creatorcontrib>Lind, K</creatorcontrib><creatorcontrib>Nordlander, T</creatorcontrib><creatorcontrib>Hansen, T T</creatorcontrib><creatorcontrib>Heger, A</creatorcontrib><title>Raising the observed metallicity floor with a 3D non-LTE analysis of SDSS J102915.14+172927.9</title><title>arXiv.org</title><description>Context: The first stars produced the first heavy elements and set the stage for the formation of the first galaxies. Accurate chemical abundances of ultra metal-poor stars ([Fe/H]<-4) can be used to infer properties of the first stars, and thus the formation mechanism for low-mass second generation stars in the early universe. Spectroscopic studies have shown that most second generation stars are carbon-enhanced with one notable exception SDSS J102915.14+172927.9. Aims: We reanalyse the composition of SDSS J102915.14+172927.9. Methods: We developed a tailored 3D model atmosphere for SDSS J102915.14+172927.9 with the Stagger-code, making use of an improved surface gravity estimate based on the Gaia DR3 parallax. This model was used as input in the radiative transfer code Balder to compute 3D non-LTE synthetic spectra. These spectra were then used to infer abundances for Mg, Si, Ca, Fe and Ni, and upper limits on Li, Na and Al. 3D LTE synthetic spectra were computed with Scate to infer the abundance of Ti and upper limits on C and N. Results: In contrast to earlier works based on 1D non-LTE corrections to 3D LTE results, we are able to achieve ionisation balance for Ca I and Ca II when employing our consistent 3D non-LTE treatment. Moreover, the elemental abundances are systematically higher than those found in earlier works. In particular, [Fe/H] increases by 0.57 dex, and the upper limits of C and N increase by 0.90 dex and 1.82 dex, respectively. Conclusions: We find that Population III progenitors with masses 10-20 M_sun exploding with energy E<=3*10^{51} erg can reproduce our 3D non-LTE abundance pattern. Contrary to previous work, we obtain higher upper limits on the carbon abundance that are ``marginally consistent'' with star formation through atomic line cooling, and as such, prevent strong conclusions about the formation mechanism of this low mass star.</description><subject>Abundance</subject><subject>Calcium</subject><subject>Carbon</subject><subject>Galaxies</subject><subject>Heavy elements</subject><subject>Iron</subject><subject>Low mass stars</subject><subject>Metallicity</subject><subject>Parallax</subject><subject>Physics - Astrophysics of Galaxies</subject><subject>Physics - Solar and Stellar Astrophysics</subject><subject>Radiative transfer</subject><subject>Spectra</subject><subject>Star & galaxy formation</subject><subject>Star formation</subject><subject>Three dimensional models</subject><subject>Titanium</subject><issn>2331-8422</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2023</creationdate><recordtype>article</recordtype><sourceid>ABUWG</sourceid><sourceid>AFKRA</sourceid><sourceid>AZQEC</sourceid><sourceid>BENPR</sourceid><sourceid>CCPQU</sourceid><sourceid>DWQXO</sourceid><sourceid>GOX</sourceid><recordid>eNotkMFKAzEYhIMgWGofwJMBj7Jrkj_ZbI7S1qoUBNurLEmTtSnbTU221b69a-tp5jAM8w1CN5TkvBSCPOj44w85AwI5oSD5BRowAJqVnLErNEppQwhhhWRCwAB9vGuffPuJu7XDwSQXD87iret00_iV7464bkKI-Nt3a6wxTHAb2my-nGLd6uaYfMKhxovJYoFfKWGKipzyeyqZYjJX1-iy1k1yo38douXTdDl-zuZvs5fx4zzTSvBsRRhYVhRgV5IaJ3trua2NclYLYZxWUNSFMmU_W0tNwRTOWkIN1KUxUsIQ3Z5rT-zVLvqtjsfq74Pq9EGfuDsndjF87V3qqk3Yx54gVUyWjFAGlMMvsgdbWw</recordid><startdate>20230302</startdate><enddate>20230302</enddate><creator>Lagae, C</creator><creator>Amarsi, A M</creator><creator>Rodríguez Díaz, L F</creator><creator>Lind, K</creator><creator>Nordlander, T</creator><creator>Hansen, T T</creator><creator>Heger, A</creator><general>Cornell University Library, arXiv.org</general><scope>8FE</scope><scope>8FG</scope><scope>ABJCF</scope><scope>ABUWG</scope><scope>AFKRA</scope><scope>AZQEC</scope><scope>BENPR</scope><scope>BGLVJ</scope><scope>CCPQU</scope><scope>DWQXO</scope><scope>HCIFZ</scope><scope>L6V</scope><scope>M7S</scope><scope>PIMPY</scope><scope>PQEST</scope><scope>PQQKQ</scope><scope>PQUKI</scope><scope>PRINS</scope><scope>PTHSS</scope><scope>GOX</scope></search><sort><creationdate>20230302</creationdate><title>Raising the observed metallicity floor with a 3D non-LTE analysis of SDSS J102915.14+172927.9</title><author>Lagae, C ; Amarsi, A M ; Rodríguez Díaz, L F ; Lind, K ; Nordlander, T ; Hansen, T T ; Heger, A</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-a954-c023d2663dc71be7266d4dfb9eda55bea936f69b8026a7a13b6edd01b3f8bb773</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2023</creationdate><topic>Abundance</topic><topic>Calcium</topic><topic>Carbon</topic><topic>Galaxies</topic><topic>Heavy elements</topic><topic>Iron</topic><topic>Low mass stars</topic><topic>Metallicity</topic><topic>Parallax</topic><topic>Physics - Astrophysics of Galaxies</topic><topic>Physics - Solar and Stellar Astrophysics</topic><topic>Radiative transfer</topic><topic>Spectra</topic><topic>Star & galaxy formation</topic><topic>Star formation</topic><topic>Three dimensional models</topic><topic>Titanium</topic><toplevel>online_resources</toplevel><creatorcontrib>Lagae, C</creatorcontrib><creatorcontrib>Amarsi, A M</creatorcontrib><creatorcontrib>Rodríguez Díaz, L F</creatorcontrib><creatorcontrib>Lind, K</creatorcontrib><creatorcontrib>Nordlander, T</creatorcontrib><creatorcontrib>Hansen, T T</creatorcontrib><creatorcontrib>Heger, A</creatorcontrib><collection>ProQuest SciTech Collection</collection><collection>ProQuest Technology Collection</collection><collection>Materials Science & Engineering Collection</collection><collection>ProQuest Central (Alumni Edition)</collection><collection>ProQuest Central UK/Ireland</collection><collection>ProQuest Central Essentials</collection><collection>ProQuest Central</collection><collection>Technology Collection</collection><collection>ProQuest One Community College</collection><collection>ProQuest Central Korea</collection><collection>SciTech Premium Collection</collection><collection>ProQuest Engineering Collection</collection><collection>Engineering Database</collection><collection>Publicly Available Content Database</collection><collection>ProQuest One Academic Eastern Edition (DO NOT USE)</collection><collection>ProQuest One Academic</collection><collection>ProQuest One Academic UKI Edition</collection><collection>ProQuest Central China</collection><collection>Engineering Collection</collection><collection>arXiv.org</collection><jtitle>arXiv.org</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Lagae, C</au><au>Amarsi, A M</au><au>Rodríguez Díaz, L F</au><au>Lind, K</au><au>Nordlander, T</au><au>Hansen, T T</au><au>Heger, A</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Raising the observed metallicity floor with a 3D non-LTE analysis of SDSS J102915.14+172927.9</atitle><jtitle>arXiv.org</jtitle><date>2023-03-02</date><risdate>2023</risdate><eissn>2331-8422</eissn><abstract>Context: The first stars produced the first heavy elements and set the stage for the formation of the first galaxies. Accurate chemical abundances of ultra metal-poor stars ([Fe/H]<-4) can be used to infer properties of the first stars, and thus the formation mechanism for low-mass second generation stars in the early universe. Spectroscopic studies have shown that most second generation stars are carbon-enhanced with one notable exception SDSS J102915.14+172927.9. Aims: We reanalyse the composition of SDSS J102915.14+172927.9. Methods: We developed a tailored 3D model atmosphere for SDSS J102915.14+172927.9 with the Stagger-code, making use of an improved surface gravity estimate based on the Gaia DR3 parallax. This model was used as input in the radiative transfer code Balder to compute 3D non-LTE synthetic spectra. These spectra were then used to infer abundances for Mg, Si, Ca, Fe and Ni, and upper limits on Li, Na and Al. 3D LTE synthetic spectra were computed with Scate to infer the abundance of Ti and upper limits on C and N. Results: In contrast to earlier works based on 1D non-LTE corrections to 3D LTE results, we are able to achieve ionisation balance for Ca I and Ca II when employing our consistent 3D non-LTE treatment. Moreover, the elemental abundances are systematically higher than those found in earlier works. In particular, [Fe/H] increases by 0.57 dex, and the upper limits of C and N increase by 0.90 dex and 1.82 dex, respectively. Conclusions: We find that Population III progenitors with masses 10-20 M_sun exploding with energy E<=3*10^{51} erg can reproduce our 3D non-LTE abundance pattern. Contrary to previous work, we obtain higher upper limits on the carbon abundance that are ``marginally consistent'' with star formation through atomic line cooling, and as such, prevent strong conclusions about the formation mechanism of this low mass star.</abstract><cop>Ithaca</cop><pub>Cornell University Library, arXiv.org</pub><doi>10.48550/arxiv.2303.01374</doi><oa>free_for_read</oa></addata></record> |
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| subjects | Abundance Calcium Carbon Galaxies Heavy elements Iron Low mass stars Metallicity Parallax Physics - Astrophysics of Galaxies Physics - Solar and Stellar Astrophysics Radiative transfer Spectra Star & galaxy formation Star formation Three dimensional models Titanium |
| title | Raising the observed metallicity floor with a 3D non-LTE analysis of SDSS J102915.14+172927.9 |
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