J0023+0307: A Mega Metal-poor Dwarf Star from SDSS/BOSS
Only a handful of stars have been identified with an iron abundance [Fe/H]
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| Veröffentlicht in: | Astrophysical journal. Letters 2018-02, Vol.854 (2), p.L34 |
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| container_issue | 2 |
| container_start_page | L34 |
| container_title | Astrophysical journal. Letters |
| container_volume | 854 |
| creator | Aguado, David S. Prieto, Carlos Allende Hernández, Jonay I. González Rebolo, Rafael |
| description | Only a handful of stars have been identified with an iron abundance [Fe/H] |
| doi_str_mv | 10.3847/2041-8213/aaadb8 |
| format | Article |
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∼ 7.0, most likely due to fallback in core-collapse supernovae, which makes their total metallicity
Z
much higher than their iron abundances. The failure to find population III stars, those with no metals, has been interpreted, with support from theoretical modeling, as the result of a top-heavy initial mass function. With zero or very low metal abundance limiting radiative cooling, the formation of low-mass stars could be inhibited. Currently, the star SDSS J1029+1729 sets the potential metallicity threshold for the formation of low-mass stars at
. In our quest to push down the metallicity threshold we have identified SDSS J0023+0307, a primitive star with
T
eff
= 6188 ± 84 K, and
, an upper limit [Fe/H] < −6.6, and a carbon abundance
A
(
C
) < 6.3. We find J0023+0307 to be one of the two most iron-poor stars known, and it exhibits less carbon that most of the stars at [Fe/H] < −5.</description><identifier>ISSN: 2041-8205</identifier><identifier>EISSN: 2041-8213</identifier><identifier>DOI: 10.3847/2041-8213/aaadb8</identifier><language>eng</language><publisher>Austin: IOP Publishing</publisher><subject>Abundance ; Carbon ; Core making ; Dwarf stars ; Initial mass function ; Iron ; Low mass stars ; Metallicity ; Population III stars ; Radiative cooling ; Supernovae</subject><ispartof>Astrophysical journal. Letters, 2018-02, Vol.854 (2), p.L34</ispartof><rights>Copyright IOP Publishing Feb 20, 2018</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c379t-15f1e9db32c157fb14664a9c267b0b14c267932130591c2cf0eedce5fc330b953</citedby><cites>FETCH-LOGICAL-c379t-15f1e9db32c157fb14664a9c267b0b14c267932130591c2cf0eedce5fc330b953</cites><orcidid>0000-0001-5200-3973 ; 0000-0003-3767-7085 ; 0000-0002-0264-7356 ; 0000-0002-0084-572X</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>314,780,784,27923,27924</link.rule.ids></links><search><creatorcontrib>Aguado, David S.</creatorcontrib><creatorcontrib>Prieto, Carlos Allende</creatorcontrib><creatorcontrib>Hernández, Jonay I. González</creatorcontrib><creatorcontrib>Rebolo, Rafael</creatorcontrib><title>J0023+0307: A Mega Metal-poor Dwarf Star from SDSS/BOSS</title><title>Astrophysical journal. Letters</title><description>Only a handful of stars have been identified with an iron abundance [Fe/H] < −5, and only one at [Fe/H] < −7. These stars have very large carbon-to-iron ratios, with
∼ 7.0, most likely due to fallback in core-collapse supernovae, which makes their total metallicity
Z
much higher than their iron abundances. The failure to find population III stars, those with no metals, has been interpreted, with support from theoretical modeling, as the result of a top-heavy initial mass function. With zero or very low metal abundance limiting radiative cooling, the formation of low-mass stars could be inhibited. Currently, the star SDSS J1029+1729 sets the potential metallicity threshold for the formation of low-mass stars at
. In our quest to push down the metallicity threshold we have identified SDSS J0023+0307, a primitive star with
T
eff
= 6188 ± 84 K, and
, an upper limit [Fe/H] < −6.6, and a carbon abundance
A
(
C
) < 6.3. We find J0023+0307 to be one of the two most iron-poor stars known, and it exhibits less carbon that most of the stars at [Fe/H] < −5.</description><subject>Abundance</subject><subject>Carbon</subject><subject>Core making</subject><subject>Dwarf stars</subject><subject>Initial mass function</subject><subject>Iron</subject><subject>Low mass stars</subject><subject>Metallicity</subject><subject>Population III stars</subject><subject>Radiative cooling</subject><subject>Supernovae</subject><issn>2041-8205</issn><issn>2041-8213</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2018</creationdate><recordtype>article</recordtype><recordid>eNo9UE1LAzEQDaJgrd49BjzKupNkk2y81dZPKj2snkM2m4ilNWuyRfz3Zqn0MvNmeMyb9xC6JHDD6kqWFCpS1JSw0hjTtfURmhxWxwcM_BSdpbQGoCBIPUHyJUN2DQzkLZ7hV_dhchnMpuhDiHjxY6LHzWAi9jFscbNomvJu1TTn6MSbTXIX_32K3h_u3-ZPxXL1-DyfLQvLpBoKwj1xqmsZtYRL35JKiMooS4VsIU8jUCy_CFwRS60H5zrruLeMQas4m6Kr_d0-hu-dS4Neh138ypKaMsGFINlHZsGeZWNIKTqv-_i5NfFXE9BjPHr0r8cs9D4e9ge9HVO0</recordid><startdate>20180220</startdate><enddate>20180220</enddate><creator>Aguado, David S.</creator><creator>Prieto, Carlos Allende</creator><creator>Hernández, Jonay I. González</creator><creator>Rebolo, Rafael</creator><general>IOP Publishing</general><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>8FD</scope><scope>H8D</scope><scope>KL.</scope><scope>L7M</scope><orcidid>https://orcid.org/0000-0001-5200-3973</orcidid><orcidid>https://orcid.org/0000-0003-3767-7085</orcidid><orcidid>https://orcid.org/0000-0002-0264-7356</orcidid><orcidid>https://orcid.org/0000-0002-0084-572X</orcidid></search><sort><creationdate>20180220</creationdate><title>J0023+0307: A Mega Metal-poor Dwarf Star from SDSS/BOSS</title><author>Aguado, David S. ; Prieto, Carlos Allende ; Hernández, Jonay I. González ; Rebolo, Rafael</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c379t-15f1e9db32c157fb14664a9c267b0b14c267932130591c2cf0eedce5fc330b953</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2018</creationdate><topic>Abundance</topic><topic>Carbon</topic><topic>Core making</topic><topic>Dwarf stars</topic><topic>Initial mass function</topic><topic>Iron</topic><topic>Low mass stars</topic><topic>Metallicity</topic><topic>Population III stars</topic><topic>Radiative cooling</topic><topic>Supernovae</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Aguado, David S.</creatorcontrib><creatorcontrib>Prieto, Carlos Allende</creatorcontrib><creatorcontrib>Hernández, Jonay I. González</creatorcontrib><creatorcontrib>Rebolo, Rafael</creatorcontrib><collection>CrossRef</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><collection>Advanced Technologies Database with Aerospace</collection><jtitle>Astrophysical journal. Letters</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Aguado, David S.</au><au>Prieto, Carlos Allende</au><au>Hernández, Jonay I. González</au><au>Rebolo, Rafael</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>J0023+0307: A Mega Metal-poor Dwarf Star from SDSS/BOSS</atitle><jtitle>Astrophysical journal. Letters</jtitle><date>2018-02-20</date><risdate>2018</risdate><volume>854</volume><issue>2</issue><spage>L34</spage><pages>L34-</pages><issn>2041-8205</issn><eissn>2041-8213</eissn><abstract>Only a handful of stars have been identified with an iron abundance [Fe/H] < −5, and only one at [Fe/H] < −7. These stars have very large carbon-to-iron ratios, with
∼ 7.0, most likely due to fallback in core-collapse supernovae, which makes their total metallicity
Z
much higher than their iron abundances. The failure to find population III stars, those with no metals, has been interpreted, with support from theoretical modeling, as the result of a top-heavy initial mass function. With zero or very low metal abundance limiting radiative cooling, the formation of low-mass stars could be inhibited. Currently, the star SDSS J1029+1729 sets the potential metallicity threshold for the formation of low-mass stars at
. In our quest to push down the metallicity threshold we have identified SDSS J0023+0307, a primitive star with
T
eff
= 6188 ± 84 K, and
, an upper limit [Fe/H] < −6.6, and a carbon abundance
A
(
C
) < 6.3. We find J0023+0307 to be one of the two most iron-poor stars known, and it exhibits less carbon that most of the stars at [Fe/H] < −5.</abstract><cop>Austin</cop><pub>IOP Publishing</pub><doi>10.3847/2041-8213/aaadb8</doi><orcidid>https://orcid.org/0000-0001-5200-3973</orcidid><orcidid>https://orcid.org/0000-0003-3767-7085</orcidid><orcidid>https://orcid.org/0000-0002-0264-7356</orcidid><orcidid>https://orcid.org/0000-0002-0084-572X</orcidid><oa>free_for_read</oa></addata></record> |
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| source | IOP Publishing Free Content; EZB-FREE-00999 freely available EZB journals; IOPscience extra; Alma/SFX Local Collection |
| subjects | Abundance Carbon Core making Dwarf stars Initial mass function Iron Low mass stars Metallicity Population III stars Radiative cooling Supernovae |
| title | J0023+0307: A Mega Metal-poor Dwarf Star from SDSS/BOSS |
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