A Chemical Composition Survey of the Iron-complex Globular Cluster NGC 6273 (M19)
Recent observations have shown that a growing number of the most massive Galactic globular clusters contain multiple populations of stars with different [Fe/H] and neutron-capture element abundances. NGC 6273 has only recently been recognized as a member of this “iron-complex” cluster class, and we...
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| Veröffentlicht in: | The Astrophysical journal 2017-02, Vol.836 (2), p.168 |
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| creator | Johnson, Christian I. Caldwell, Nelson Rich, R. Michael Mateo, Mario Bailey, III, John I. Clarkson, William I. Olszewski, Edward W. Walker, Matthew G. |
| description | Recent observations have shown that a growing number of the most massive Galactic globular clusters contain multiple populations of stars with different [Fe/H] and neutron-capture element abundances. NGC 6273 has only recently been recognized as a member of this “iron-complex” cluster class, and we provide here a chemical and kinematic analysis of >300 red giant branch and asymptotic giant branch member stars using high-resolution spectra obtained with the
Magellan
–M2FS and VLT–FLAMES instruments. Multiple lines of evidence indicate that NGC 6273 possesses an intrinsic metallicity spread that ranges from about [Fe/H] = −2 to −1 dex, and may include at least three populations with different [Fe/H] values. The three populations identified here contain separate first (Na/Al-poor) and second (Na/Al-rich) generation stars, but a Mg–Al anti-correlation may only be present in stars with [Fe/H] ≳ −1.65. The strong correlation between [La/Eu] and [Fe/H] suggests that the s-process must have dominated the heavy element enrichment at higher metallicities. A small group of stars with low [
α
/Fe] is identified and may have been accreted from a former surrounding field star population. The cluster’s large abundance variations are coupled with a complex, extended, and multimodal blue horizontal branch (HB). The HB morphology and chemical abundances suggest that NGC 6273 may have an origin that is similar to
ω
Cen and M54. |
| doi_str_mv | 10.3847/1538-4357/836/2/168 |
| format | Article |
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Magellan
–M2FS and VLT–FLAMES instruments. Multiple lines of evidence indicate that NGC 6273 possesses an intrinsic metallicity spread that ranges from about [Fe/H] = −2 to −1 dex, and may include at least three populations with different [Fe/H] values. The three populations identified here contain separate first (Na/Al-poor) and second (Na/Al-rich) generation stars, but a Mg–Al anti-correlation may only be present in stars with [Fe/H] ≳ −1.65. The strong correlation between [La/Eu] and [Fe/H] suggests that the s-process must have dominated the heavy element enrichment at higher metallicities. A small group of stars with low [
α
/Fe] is identified and may have been accreted from a former surrounding field star population. The cluster’s large abundance variations are coupled with a complex, extended, and multimodal blue horizontal branch (HB). The HB morphology and chemical abundances suggest that NGC 6273 may have an origin that is similar to
ω
Cen and M54.</description><identifier>ISSN: 0004-637X</identifier><identifier>EISSN: 1538-4357</identifier><identifier>DOI: 10.3847/1538-4357/836/2/168</identifier><language>eng</language><publisher>Philadelphia: IOP Publishing</publisher><subject>Abundance ; Aluminum ; Astrophysics ; ASTROPHYSICS, COSMOLOGY AND ASTRONOMY ; ASYMPTOTIC SOLUTIONS ; CAPTURE ; Chemical composition ; Correlation ; CORRELATIONS ; ELEMENT ABUNDANCE ; ENRICHMENT ; FLAMES ; Globular clusters ; Heavy elements ; IRON ; Magnesium ; METALLICITY ; Morphology ; NEUTRON REACTIONS ; Nuclear capture ; Organic chemistry ; Populations ; Red giant stars ; RESOLUTION ; S PROCESS ; SPECTRA ; STAR EVOLUTION ; STARS</subject><ispartof>The Astrophysical journal, 2017-02, Vol.836 (2), p.168</ispartof><rights>Copyright IOP Publishing Feb 20, 2017</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c350t-dd0cf7fbaaaf83f83515de1e0c97149957304045d4d3b4a252affbfa8d3e4ce43</citedby><cites>FETCH-LOGICAL-c350t-dd0cf7fbaaaf83f83515de1e0c97149957304045d4d3b4a252affbfa8d3e4ce43</cites><orcidid>0000-0003-2496-1925 ; 0000-0002-8878-3315 ; 0000-0003-2352-3202</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>230,314,780,784,885,27924,27925</link.rule.ids><backlink>$$Uhttps://www.osti.gov/biblio/22663781$$D View this record in Osti.gov$$Hfree_for_read</backlink></links><search><creatorcontrib>Johnson, Christian I.</creatorcontrib><creatorcontrib>Caldwell, Nelson</creatorcontrib><creatorcontrib>Rich, R. Michael</creatorcontrib><creatorcontrib>Mateo, Mario</creatorcontrib><creatorcontrib>Bailey, III, John I.</creatorcontrib><creatorcontrib>Clarkson, William I.</creatorcontrib><creatorcontrib>Olszewski, Edward W.</creatorcontrib><creatorcontrib>Walker, Matthew G.</creatorcontrib><title>A Chemical Composition Survey of the Iron-complex Globular Cluster NGC 6273 (M19)</title><title>The Astrophysical journal</title><description>Recent observations have shown that a growing number of the most massive Galactic globular clusters contain multiple populations of stars with different [Fe/H] and neutron-capture element abundances. NGC 6273 has only recently been recognized as a member of this “iron-complex” cluster class, and we provide here a chemical and kinematic analysis of >300 red giant branch and asymptotic giant branch member stars using high-resolution spectra obtained with the
Magellan
–M2FS and VLT–FLAMES instruments. Multiple lines of evidence indicate that NGC 6273 possesses an intrinsic metallicity spread that ranges from about [Fe/H] = −2 to −1 dex, and may include at least three populations with different [Fe/H] values. The three populations identified here contain separate first (Na/Al-poor) and second (Na/Al-rich) generation stars, but a Mg–Al anti-correlation may only be present in stars with [Fe/H] ≳ −1.65. The strong correlation between [La/Eu] and [Fe/H] suggests that the s-process must have dominated the heavy element enrichment at higher metallicities. A small group of stars with low [
α
/Fe] is identified and may have been accreted from a former surrounding field star population. The cluster’s large abundance variations are coupled with a complex, extended, and multimodal blue horizontal branch (HB). The HB morphology and chemical abundances suggest that NGC 6273 may have an origin that is similar to
ω
Cen and M54.</description><subject>Abundance</subject><subject>Aluminum</subject><subject>Astrophysics</subject><subject>ASTROPHYSICS, COSMOLOGY AND ASTRONOMY</subject><subject>ASYMPTOTIC SOLUTIONS</subject><subject>CAPTURE</subject><subject>Chemical composition</subject><subject>Correlation</subject><subject>CORRELATIONS</subject><subject>ELEMENT ABUNDANCE</subject><subject>ENRICHMENT</subject><subject>FLAMES</subject><subject>Globular clusters</subject><subject>Heavy elements</subject><subject>IRON</subject><subject>Magnesium</subject><subject>METALLICITY</subject><subject>Morphology</subject><subject>NEUTRON REACTIONS</subject><subject>Nuclear capture</subject><subject>Organic chemistry</subject><subject>Populations</subject><subject>Red giant stars</subject><subject>RESOLUTION</subject><subject>S PROCESS</subject><subject>SPECTRA</subject><subject>STAR EVOLUTION</subject><subject>STARS</subject><issn>0004-637X</issn><issn>1538-4357</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2017</creationdate><recordtype>article</recordtype><recordid>eNpFkFFLwzAQgIMoOKe_wJeAL_pQl-SSNn0cRedgKqKCbyFNE9bRNTNpxf17WyYKB8fdfRx3H0KXlNyC5NmMCpAJB5HNJKQzNqOpPEKTv-4xmhBCeJJC9nGKzmLcjCXL8wl6meNibbe10Q0u_HbnY93VvsWvffiye-wd7tYWL4NvEzOMG_uNF40v-0YHXDR97GzAT4sCpywDfP1I85tzdOJ0E-3Fb56i9_u7t-IhWT0vlsV8lRgQpEuqihiXuVJr7SQMIaioLLXE5BnleS4yIJxwUfEKSq6ZYNq50mlZgeXGcpiiq8NeH7taRVN31qyNb1trOsVYOjwr6T-1C_6zt7FTG9-HdjhMMUiFBEYpGyg4UCb4GIN1ahfqrQ57RYkaDavRpRpdqsGwYmowDD9O3mvI</recordid><startdate>20170220</startdate><enddate>20170220</enddate><creator>Johnson, Christian I.</creator><creator>Caldwell, Nelson</creator><creator>Rich, R. 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Michael</creatorcontrib><creatorcontrib>Mateo, Mario</creatorcontrib><creatorcontrib>Bailey, III, John I.</creatorcontrib><creatorcontrib>Clarkson, William I.</creatorcontrib><creatorcontrib>Olszewski, Edward W.</creatorcontrib><creatorcontrib>Walker, Matthew G.</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><collection>OSTI.GOV</collection><jtitle>The Astrophysical journal</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Johnson, Christian I.</au><au>Caldwell, Nelson</au><au>Rich, R. Michael</au><au>Mateo, Mario</au><au>Bailey, III, John I.</au><au>Clarkson, William I.</au><au>Olszewski, Edward W.</au><au>Walker, Matthew G.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>A Chemical Composition Survey of the Iron-complex Globular Cluster NGC 6273 (M19)</atitle><jtitle>The Astrophysical journal</jtitle><date>2017-02-20</date><risdate>2017</risdate><volume>836</volume><issue>2</issue><spage>168</spage><pages>168-</pages><issn>0004-637X</issn><eissn>1538-4357</eissn><abstract>Recent observations have shown that a growing number of the most massive Galactic globular clusters contain multiple populations of stars with different [Fe/H] and neutron-capture element abundances. NGC 6273 has only recently been recognized as a member of this “iron-complex” cluster class, and we provide here a chemical and kinematic analysis of >300 red giant branch and asymptotic giant branch member stars using high-resolution spectra obtained with the
Magellan
–M2FS and VLT–FLAMES instruments. Multiple lines of evidence indicate that NGC 6273 possesses an intrinsic metallicity spread that ranges from about [Fe/H] = −2 to −1 dex, and may include at least three populations with different [Fe/H] values. The three populations identified here contain separate first (Na/Al-poor) and second (Na/Al-rich) generation stars, but a Mg–Al anti-correlation may only be present in stars with [Fe/H] ≳ −1.65. The strong correlation between [La/Eu] and [Fe/H] suggests that the s-process must have dominated the heavy element enrichment at higher metallicities. A small group of stars with low [
α
/Fe] is identified and may have been accreted from a former surrounding field star population. The cluster’s large abundance variations are coupled with a complex, extended, and multimodal blue horizontal branch (HB). The HB morphology and chemical abundances suggest that NGC 6273 may have an origin that is similar to
ω
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| source | Institute of Physics Open Access Journal Titles; EZB-FREE-00999 freely available EZB journals; Alma/SFX Local Collection |
| subjects | Abundance Aluminum Astrophysics ASTROPHYSICS, COSMOLOGY AND ASTRONOMY ASYMPTOTIC SOLUTIONS CAPTURE Chemical composition Correlation CORRELATIONS ELEMENT ABUNDANCE ENRICHMENT FLAMES Globular clusters Heavy elements IRON Magnesium METALLICITY Morphology NEUTRON REACTIONS Nuclear capture Organic chemistry Populations Red giant stars RESOLUTION S PROCESS SPECTRA STAR EVOLUTION STARS |
| title | A Chemical Composition Survey of the Iron-complex Globular Cluster NGC 6273 (M19) |
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