Impact history of the Apollo 17 landing site revealed by U‐Pb SIMS ages

Secondary ion mass spectrometry ( SIMS ) U‐Pb ages of Ca‐phosphates from four texturally distinct breccia samples (72255, 76055, 76015, 76215) collected at the Apollo 17 landing site were obtained in an attempt to identify whether they represent a single or several impact event(s). The determined ag...
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Autor*in:	Thiessen, Fiona [verfasserIn] Nemchin, Alexander A Snape, Joshua F Whitehouse, Martin J Bellucci, Jeremy J

Format:	Artikel
Sprache:	Englisch

Erschienen:	2017

Rechteinformationen:	Nutzungsrecht: © The Meteoritical Society, 2017.

Übergeordnetes Werk:	Enthalten in: Meteoritics & planetary science - Lawrence, Kan. : Allen Press, 1996, 52(2017), 4, Seite 584-611
Übergeordnetes Werk:	volume:52 ; year:2017 ; number:4 ; pages:584-611

Links:	Volltext Link aufrufen Link aufrufen

DOI / URN:	10.1111/maps.12814

Katalog-ID:	OLC1992238642

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520			\|a Secondary ion mass spectrometry ( SIMS ) U‐Pb ages of Ca‐phosphates from four texturally distinct breccia samples (72255, 76055, 76015, 76215) collected at the Apollo 17 landing site were obtained in an attempt to identify whether they represent a single or several impact event(s). The determined ages, combined with inferences from petrologic relationships, may indicate two or possibly three different impact events at 3920 ± 3 Ma, 3922 ± 5 Ma, and 3930 ± 5 Ma (all errors 2σ). Searching for possible sources of the breccias by calculating the continuous ejecta radii of impact basins and large craters as well as their expected ejecta thicknesses, we conclude that Nectaris, Crisium, Serenitatis, and Imbrium are likely candidates. If the previous interpretation that the micropoikilitic breccias collected at the North Massif represent Serenitatis ejecta is correct, then the average 207 Pb/ 206 Pb age of 3930 ± 5 Ma (2σ) dates the formation of the Serenitatis basin. The occurrence of zircon in the breccias sampled at the South Massif, which contain Ca‐phosphates yielding an age of 3922 ± 5 Ma (2σ), may indicate that the breccia originated from within the Procellarum KREEP terrane ( PKT ) and the Imbrium basin appears to be the only basin that could have sourced them. However, this interpretation implies that all basins suggested to fall stratigraphically between Serenitatis and Imbrium formed within a short (<11 Ma) time interval, highlighting serious contradictions between global stratigraphic constraints, sample interpretation, and chronological data. Alternatively, the slightly older age of the two micropoikilitic breccias may be a result of incomplete resetting of the U‐Pb system preserved in some phosphate grains. Based on the currently available data set this possibility cannot be excluded.
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allfields	10.1111/maps.12814 doi PQ20170501 (DE-627)OLC1992238642 (DE-599)GBVOLC1992238642 (PRQ)p1284-88ec88dbcfdb76f33ac633eaa1b57539548fe40dfed7cd427fe708f65e25e8f80 (KEY)0042930920170000052000400584impacthistoryoftheapollo17landingsiterevealedbyupb DE-627 ger DE-627 rakwb eng 520 550 DNB Thiessen, Fiona verfasserin aut Impact history of the Apollo 17 landing site revealed by U‐Pb SIMS ages 2017 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier Secondary ion mass spectrometry ( SIMS ) U‐Pb ages of Ca‐phosphates from four texturally distinct breccia samples (72255, 76055, 76015, 76215) collected at the Apollo 17 landing site were obtained in an attempt to identify whether they represent a single or several impact event(s). The determined ages, combined with inferences from petrologic relationships, may indicate two or possibly three different impact events at 3920 ± 3 Ma, 3922 ± 5 Ma, and 3930 ± 5 Ma (all errors 2σ). Searching for possible sources of the breccias by calculating the continuous ejecta radii of impact basins and large craters as well as their expected ejecta thicknesses, we conclude that Nectaris, Crisium, Serenitatis, and Imbrium are likely candidates. If the previous interpretation that the micropoikilitic breccias collected at the North Massif represent Serenitatis ejecta is correct, then the average 207 Pb/ 206 Pb age of 3930 ± 5 Ma (2σ) dates the formation of the Serenitatis basin. The occurrence of zircon in the breccias sampled at the South Massif, which contain Ca‐phosphates yielding an age of 3922 ± 5 Ma (2σ), may indicate that the breccia originated from within the Procellarum KREEP terrane ( PKT ) and the Imbrium basin appears to be the only basin that could have sourced them. However, this interpretation implies that all basins suggested to fall stratigraphically between Serenitatis and Imbrium formed within a short (<11 Ma) time interval, highlighting serious contradictions between global stratigraphic constraints, sample interpretation, and chronological data. Alternatively, the slightly older age of the two micropoikilitic breccias may be a result of incomplete resetting of the U‐Pb system preserved in some phosphate grains. Based on the currently available data set this possibility cannot be excluded. Nutzungsrecht: © The Meteoritical Society, 2017. Nemchin, Alexander A oth Snape, Joshua F oth Whitehouse, Martin J oth Bellucci, Jeremy J oth Enthalten in Meteoritics & planetary science Lawrence, Kan. : Allen Press, 1996 52(2017), 4, Seite 584-611 (DE-627)193298368 (DE-600)1306943-3 (DE-576)060237333 1086-9379 nnns volume:52 year:2017 number:4 pages:584-611 http://dx.doi.org/10.1111/maps.12814 Volltext http://onlinelibrary.wiley.com/doi/10.1111/maps.12814/abstract http://search.proquest.com/docview/1888562731 GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-GEO SSG-OLC-AST SSG-OPC-GGO SSG-OPC-AST GBV_ILN_2004 AR 52 2017 4 584-611
spelling	10.1111/maps.12814 doi PQ20170501 (DE-627)OLC1992238642 (DE-599)GBVOLC1992238642 (PRQ)p1284-88ec88dbcfdb76f33ac633eaa1b57539548fe40dfed7cd427fe708f65e25e8f80 (KEY)0042930920170000052000400584impacthistoryoftheapollo17landingsiterevealedbyupb DE-627 ger DE-627 rakwb eng 520 550 DNB Thiessen, Fiona verfasserin aut Impact history of the Apollo 17 landing site revealed by U‐Pb SIMS ages 2017 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier Secondary ion mass spectrometry ( SIMS ) U‐Pb ages of Ca‐phosphates from four texturally distinct breccia samples (72255, 76055, 76015, 76215) collected at the Apollo 17 landing site were obtained in an attempt to identify whether they represent a single or several impact event(s). The determined ages, combined with inferences from petrologic relationships, may indicate two or possibly three different impact events at 3920 ± 3 Ma, 3922 ± 5 Ma, and 3930 ± 5 Ma (all errors 2σ). Searching for possible sources of the breccias by calculating the continuous ejecta radii of impact basins and large craters as well as their expected ejecta thicknesses, we conclude that Nectaris, Crisium, Serenitatis, and Imbrium are likely candidates. If the previous interpretation that the micropoikilitic breccias collected at the North Massif represent Serenitatis ejecta is correct, then the average 207 Pb/ 206 Pb age of 3930 ± 5 Ma (2σ) dates the formation of the Serenitatis basin. The occurrence of zircon in the breccias sampled at the South Massif, which contain Ca‐phosphates yielding an age of 3922 ± 5 Ma (2σ), may indicate that the breccia originated from within the Procellarum KREEP terrane ( PKT ) and the Imbrium basin appears to be the only basin that could have sourced them. However, this interpretation implies that all basins suggested to fall stratigraphically between Serenitatis and Imbrium formed within a short (<11 Ma) time interval, highlighting serious contradictions between global stratigraphic constraints, sample interpretation, and chronological data. Alternatively, the slightly older age of the two micropoikilitic breccias may be a result of incomplete resetting of the U‐Pb system preserved in some phosphate grains. Based on the currently available data set this possibility cannot be excluded. Nutzungsrecht: © The Meteoritical Society, 2017. Nemchin, Alexander A oth Snape, Joshua F oth Whitehouse, Martin J oth Bellucci, Jeremy J oth Enthalten in Meteoritics & planetary science Lawrence, Kan. : Allen Press, 1996 52(2017), 4, Seite 584-611 (DE-627)193298368 (DE-600)1306943-3 (DE-576)060237333 1086-9379 nnns volume:52 year:2017 number:4 pages:584-611 http://dx.doi.org/10.1111/maps.12814 Volltext http://onlinelibrary.wiley.com/doi/10.1111/maps.12814/abstract http://search.proquest.com/docview/1888562731 GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-GEO SSG-OLC-AST SSG-OPC-GGO SSG-OPC-AST GBV_ILN_2004 AR 52 2017 4 584-611
allfields_unstemmed	10.1111/maps.12814 doi PQ20170501 (DE-627)OLC1992238642 (DE-599)GBVOLC1992238642 (PRQ)p1284-88ec88dbcfdb76f33ac633eaa1b57539548fe40dfed7cd427fe708f65e25e8f80 (KEY)0042930920170000052000400584impacthistoryoftheapollo17landingsiterevealedbyupb DE-627 ger DE-627 rakwb eng 520 550 DNB Thiessen, Fiona verfasserin aut Impact history of the Apollo 17 landing site revealed by U‐Pb SIMS ages 2017 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier Secondary ion mass spectrometry ( SIMS ) U‐Pb ages of Ca‐phosphates from four texturally distinct breccia samples (72255, 76055, 76015, 76215) collected at the Apollo 17 landing site were obtained in an attempt to identify whether they represent a single or several impact event(s). The determined ages, combined with inferences from petrologic relationships, may indicate two or possibly three different impact events at 3920 ± 3 Ma, 3922 ± 5 Ma, and 3930 ± 5 Ma (all errors 2σ). Searching for possible sources of the breccias by calculating the continuous ejecta radii of impact basins and large craters as well as their expected ejecta thicknesses, we conclude that Nectaris, Crisium, Serenitatis, and Imbrium are likely candidates. If the previous interpretation that the micropoikilitic breccias collected at the North Massif represent Serenitatis ejecta is correct, then the average 207 Pb/ 206 Pb age of 3930 ± 5 Ma (2σ) dates the formation of the Serenitatis basin. The occurrence of zircon in the breccias sampled at the South Massif, which contain Ca‐phosphates yielding an age of 3922 ± 5 Ma (2σ), may indicate that the breccia originated from within the Procellarum KREEP terrane ( PKT ) and the Imbrium basin appears to be the only basin that could have sourced them. However, this interpretation implies that all basins suggested to fall stratigraphically between Serenitatis and Imbrium formed within a short (<11 Ma) time interval, highlighting serious contradictions between global stratigraphic constraints, sample interpretation, and chronological data. Alternatively, the slightly older age of the two micropoikilitic breccias may be a result of incomplete resetting of the U‐Pb system preserved in some phosphate grains. Based on the currently available data set this possibility cannot be excluded. Nutzungsrecht: © The Meteoritical Society, 2017. Nemchin, Alexander A oth Snape, Joshua F oth Whitehouse, Martin J oth Bellucci, Jeremy J oth Enthalten in Meteoritics & planetary science Lawrence, Kan. : Allen Press, 1996 52(2017), 4, Seite 584-611 (DE-627)193298368 (DE-600)1306943-3 (DE-576)060237333 1086-9379 nnns volume:52 year:2017 number:4 pages:584-611 http://dx.doi.org/10.1111/maps.12814 Volltext http://onlinelibrary.wiley.com/doi/10.1111/maps.12814/abstract http://search.proquest.com/docview/1888562731 GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-GEO SSG-OLC-AST SSG-OPC-GGO SSG-OPC-AST GBV_ILN_2004 AR 52 2017 4 584-611
allfieldsGer	10.1111/maps.12814 doi PQ20170501 (DE-627)OLC1992238642 (DE-599)GBVOLC1992238642 (PRQ)p1284-88ec88dbcfdb76f33ac633eaa1b57539548fe40dfed7cd427fe708f65e25e8f80 (KEY)0042930920170000052000400584impacthistoryoftheapollo17landingsiterevealedbyupb DE-627 ger DE-627 rakwb eng 520 550 DNB Thiessen, Fiona verfasserin aut Impact history of the Apollo 17 landing site revealed by U‐Pb SIMS ages 2017 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier Secondary ion mass spectrometry ( SIMS ) U‐Pb ages of Ca‐phosphates from four texturally distinct breccia samples (72255, 76055, 76015, 76215) collected at the Apollo 17 landing site were obtained in an attempt to identify whether they represent a single or several impact event(s). The determined ages, combined with inferences from petrologic relationships, may indicate two or possibly three different impact events at 3920 ± 3 Ma, 3922 ± 5 Ma, and 3930 ± 5 Ma (all errors 2σ). Searching for possible sources of the breccias by calculating the continuous ejecta radii of impact basins and large craters as well as their expected ejecta thicknesses, we conclude that Nectaris, Crisium, Serenitatis, and Imbrium are likely candidates. If the previous interpretation that the micropoikilitic breccias collected at the North Massif represent Serenitatis ejecta is correct, then the average 207 Pb/ 206 Pb age of 3930 ± 5 Ma (2σ) dates the formation of the Serenitatis basin. The occurrence of zircon in the breccias sampled at the South Massif, which contain Ca‐phosphates yielding an age of 3922 ± 5 Ma (2σ), may indicate that the breccia originated from within the Procellarum KREEP terrane ( PKT ) and the Imbrium basin appears to be the only basin that could have sourced them. However, this interpretation implies that all basins suggested to fall stratigraphically between Serenitatis and Imbrium formed within a short (<11 Ma) time interval, highlighting serious contradictions between global stratigraphic constraints, sample interpretation, and chronological data. Alternatively, the slightly older age of the two micropoikilitic breccias may be a result of incomplete resetting of the U‐Pb system preserved in some phosphate grains. Based on the currently available data set this possibility cannot be excluded. Nutzungsrecht: © The Meteoritical Society, 2017. Nemchin, Alexander A oth Snape, Joshua F oth Whitehouse, Martin J oth Bellucci, Jeremy J oth Enthalten in Meteoritics & planetary science Lawrence, Kan. : Allen Press, 1996 52(2017), 4, Seite 584-611 (DE-627)193298368 (DE-600)1306943-3 (DE-576)060237333 1086-9379 nnns volume:52 year:2017 number:4 pages:584-611 http://dx.doi.org/10.1111/maps.12814 Volltext http://onlinelibrary.wiley.com/doi/10.1111/maps.12814/abstract http://search.proquest.com/docview/1888562731 GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-GEO SSG-OLC-AST SSG-OPC-GGO SSG-OPC-AST GBV_ILN_2004 AR 52 2017 4 584-611
allfieldsSound	10.1111/maps.12814 doi PQ20170501 (DE-627)OLC1992238642 (DE-599)GBVOLC1992238642 (PRQ)p1284-88ec88dbcfdb76f33ac633eaa1b57539548fe40dfed7cd427fe708f65e25e8f80 (KEY)0042930920170000052000400584impacthistoryoftheapollo17landingsiterevealedbyupb DE-627 ger DE-627 rakwb eng 520 550 DNB Thiessen, Fiona verfasserin aut Impact history of the Apollo 17 landing site revealed by U‐Pb SIMS ages 2017 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier Secondary ion mass spectrometry ( SIMS ) U‐Pb ages of Ca‐phosphates from four texturally distinct breccia samples (72255, 76055, 76015, 76215) collected at the Apollo 17 landing site were obtained in an attempt to identify whether they represent a single or several impact event(s). The determined ages, combined with inferences from petrologic relationships, may indicate two or possibly three different impact events at 3920 ± 3 Ma, 3922 ± 5 Ma, and 3930 ± 5 Ma (all errors 2σ). Searching for possible sources of the breccias by calculating the continuous ejecta radii of impact basins and large craters as well as their expected ejecta thicknesses, we conclude that Nectaris, Crisium, Serenitatis, and Imbrium are likely candidates. If the previous interpretation that the micropoikilitic breccias collected at the North Massif represent Serenitatis ejecta is correct, then the average 207 Pb/ 206 Pb age of 3930 ± 5 Ma (2σ) dates the formation of the Serenitatis basin. The occurrence of zircon in the breccias sampled at the South Massif, which contain Ca‐phosphates yielding an age of 3922 ± 5 Ma (2σ), may indicate that the breccia originated from within the Procellarum KREEP terrane ( PKT ) and the Imbrium basin appears to be the only basin that could have sourced them. However, this interpretation implies that all basins suggested to fall stratigraphically between Serenitatis and Imbrium formed within a short (<11 Ma) time interval, highlighting serious contradictions between global stratigraphic constraints, sample interpretation, and chronological data. Alternatively, the slightly older age of the two micropoikilitic breccias may be a result of incomplete resetting of the U‐Pb system preserved in some phosphate grains. Based on the currently available data set this possibility cannot be excluded. Nutzungsrecht: © The Meteoritical Society, 2017. Nemchin, Alexander A oth Snape, Joshua F oth Whitehouse, Martin J oth Bellucci, Jeremy J oth Enthalten in Meteoritics & planetary science Lawrence, Kan. : Allen Press, 1996 52(2017), 4, Seite 584-611 (DE-627)193298368 (DE-600)1306943-3 (DE-576)060237333 1086-9379 nnns volume:52 year:2017 number:4 pages:584-611 http://dx.doi.org/10.1111/maps.12814 Volltext http://onlinelibrary.wiley.com/doi/10.1111/maps.12814/abstract http://search.proquest.com/docview/1888562731 GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-GEO SSG-OLC-AST SSG-OPC-GGO SSG-OPC-AST GBV_ILN_2004 AR 52 2017 4 584-611
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author	Thiessen, Fiona
spellingShingle	Thiessen, Fiona ddc 520 Impact history of the Apollo 17 landing site revealed by U‐Pb SIMS ages
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title	Impact history of the Apollo 17 landing site revealed by U‐Pb SIMS ages
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title_sort	impact history of the apollo 17 landing site revealed by u‐pb sims ages
title_auth	Impact history of the Apollo 17 landing site revealed by U‐Pb SIMS ages
abstract	Secondary ion mass spectrometry ( SIMS ) U‐Pb ages of Ca‐phosphates from four texturally distinct breccia samples (72255, 76055, 76015, 76215) collected at the Apollo 17 landing site were obtained in an attempt to identify whether they represent a single or several impact event(s). The determined ages, combined with inferences from petrologic relationships, may indicate two or possibly three different impact events at 3920 ± 3 Ma, 3922 ± 5 Ma, and 3930 ± 5 Ma (all errors 2σ). Searching for possible sources of the breccias by calculating the continuous ejecta radii of impact basins and large craters as well as their expected ejecta thicknesses, we conclude that Nectaris, Crisium, Serenitatis, and Imbrium are likely candidates. If the previous interpretation that the micropoikilitic breccias collected at the North Massif represent Serenitatis ejecta is correct, then the average 207 Pb/ 206 Pb age of 3930 ± 5 Ma (2σ) dates the formation of the Serenitatis basin. The occurrence of zircon in the breccias sampled at the South Massif, which contain Ca‐phosphates yielding an age of 3922 ± 5 Ma (2σ), may indicate that the breccia originated from within the Procellarum KREEP terrane ( PKT ) and the Imbrium basin appears to be the only basin that could have sourced them. However, this interpretation implies that all basins suggested to fall stratigraphically between Serenitatis and Imbrium formed within a short (<11 Ma) time interval, highlighting serious contradictions between global stratigraphic constraints, sample interpretation, and chronological data. Alternatively, the slightly older age of the two micropoikilitic breccias may be a result of incomplete resetting of the U‐Pb system preserved in some phosphate grains. Based on the currently available data set this possibility cannot be excluded.
abstractGer	Secondary ion mass spectrometry ( SIMS ) U‐Pb ages of Ca‐phosphates from four texturally distinct breccia samples (72255, 76055, 76015, 76215) collected at the Apollo 17 landing site were obtained in an attempt to identify whether they represent a single or several impact event(s). The determined ages, combined with inferences from petrologic relationships, may indicate two or possibly three different impact events at 3920 ± 3 Ma, 3922 ± 5 Ma, and 3930 ± 5 Ma (all errors 2σ). Searching for possible sources of the breccias by calculating the continuous ejecta radii of impact basins and large craters as well as their expected ejecta thicknesses, we conclude that Nectaris, Crisium, Serenitatis, and Imbrium are likely candidates. If the previous interpretation that the micropoikilitic breccias collected at the North Massif represent Serenitatis ejecta is correct, then the average 207 Pb/ 206 Pb age of 3930 ± 5 Ma (2σ) dates the formation of the Serenitatis basin. The occurrence of zircon in the breccias sampled at the South Massif, which contain Ca‐phosphates yielding an age of 3922 ± 5 Ma (2σ), may indicate that the breccia originated from within the Procellarum KREEP terrane ( PKT ) and the Imbrium basin appears to be the only basin that could have sourced them. However, this interpretation implies that all basins suggested to fall stratigraphically between Serenitatis and Imbrium formed within a short (<11 Ma) time interval, highlighting serious contradictions between global stratigraphic constraints, sample interpretation, and chronological data. Alternatively, the slightly older age of the two micropoikilitic breccias may be a result of incomplete resetting of the U‐Pb system preserved in some phosphate grains. Based on the currently available data set this possibility cannot be excluded.
abstract_unstemmed	Secondary ion mass spectrometry ( SIMS ) U‐Pb ages of Ca‐phosphates from four texturally distinct breccia samples (72255, 76055, 76015, 76215) collected at the Apollo 17 landing site were obtained in an attempt to identify whether they represent a single or several impact event(s). The determined ages, combined with inferences from petrologic relationships, may indicate two or possibly three different impact events at 3920 ± 3 Ma, 3922 ± 5 Ma, and 3930 ± 5 Ma (all errors 2σ). Searching for possible sources of the breccias by calculating the continuous ejecta radii of impact basins and large craters as well as their expected ejecta thicknesses, we conclude that Nectaris, Crisium, Serenitatis, and Imbrium are likely candidates. If the previous interpretation that the micropoikilitic breccias collected at the North Massif represent Serenitatis ejecta is correct, then the average 207 Pb/ 206 Pb age of 3930 ± 5 Ma (2σ) dates the formation of the Serenitatis basin. The occurrence of zircon in the breccias sampled at the South Massif, which contain Ca‐phosphates yielding an age of 3922 ± 5 Ma (2σ), may indicate that the breccia originated from within the Procellarum KREEP terrane ( PKT ) and the Imbrium basin appears to be the only basin that could have sourced them. However, this interpretation implies that all basins suggested to fall stratigraphically between Serenitatis and Imbrium formed within a short (<11 Ma) time interval, highlighting serious contradictions between global stratigraphic constraints, sample interpretation, and chronological data. Alternatively, the slightly older age of the two micropoikilitic breccias may be a result of incomplete resetting of the U‐Pb system preserved in some phosphate grains. Based on the currently available data set this possibility cannot be excluded.
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title_short	Impact history of the Apollo 17 landing site revealed by U‐Pb SIMS ages
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