A DYNAMICAL SIGNATURE OF MULTIPLE STELLAR POPULATIONS IN 47 TUCANAE

Based on the width of its main sequence, and an actual observed split when viewed through particular filters, it is widely accepted that 47 Tucanae contains multiple stellar populations. In this contribution, we divide the main sequence of 47 Tuc into four color groups, which presumably represent st...

Full description

Saved in:
Bibliographic Details
Published in:Astrophysical journal. Letters 2013-07, Vol.771 (1), p.1-5
Main Authors: Richer, Harvey B, Heyl, Jeremy, Anderson, Jay, Kalirai, Jason S, Shara, Michael M, Dotter, Aaron, Fahlman, Gregory G, Rich, R Michael
Format: Article
Language:English
Subjects:
ANISOTROPY
ASTRONOMY
ASTROPHYSICS
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
CHEMICAL COMPOSITION
Color
Frames
HERTZSPRUNG-RUSSELL DIAGRAM
Kinematics
MAGELLANIC CLOUDS
MAIN SEQUENCE STARS
OPTICAL FILTERS
PROPER MOTION
RED GIANT STARS
Signatures
Stars
Stellar populations
Citations: Items that this one cites
Items that cite this one
Online Access:Get full text
Tags: Add Tag
No Tags, Be the first to tag this record!
cited_by cdi_FETCH-LOGICAL-c454t-9ec9ef672736d626058914ee1979f2ab5725f2fc36c28f9699e1dc32f5af36f93
cites cdi_FETCH-LOGICAL-c454t-9ec9ef672736d626058914ee1979f2ab5725f2fc36c28f9699e1dc32f5af36f93
container_end_page 5
container_issue 1
container_start_page 1
container_title Astrophysical journal. Letters
container_volume 771
creator Richer, Harvey B
Heyl, Jeremy
Anderson, Jay
Kalirai, Jason S
Shara, Michael M
Dotter, Aaron
Fahlman, Gregory G
Rich, R Michael
description Based on the width of its main sequence, and an actual observed split when viewed through particular filters, it is widely accepted that 47 Tucanae contains multiple stellar populations. In this contribution, we divide the main sequence of 47 Tuc into four color groups, which presumably represent stars of various chemical compositions. The kinematic properties of each of these groups are explored via proper motions, and a strong signal emerges of differing proper-motion anisotropies with differing main-sequence color; the bluest main-sequence stars exhibit the largest proper-motion anisotropy which becomes undetectable for the reddest stars. In addition, the bluest stars are also the most centrally concentrated. A similar analysis for Small Magellanic Cloud stars, which are located in the background of 47 Tuc on our frames, yields none of the anisotropy exhibited by the 47 Tuc stars. We discuss implications of these results for possible formation scenarios of the various populations.
doi_str_mv 10.1088/2041-8205/771/1/L15
format article
fullrecord <record><control><sourceid>proquest_osti_</sourceid><recordid>TN_cdi_osti_scitechconnect_22118713</recordid><sourceformat>XML</sourceformat><sourcesystem>PC</sourcesystem><sourcerecordid>1669886226</sourcerecordid><originalsourceid>FETCH-LOGICAL-c454t-9ec9ef672736d626058914ee1979f2ab5725f2fc36c28f9699e1dc32f5af36f93</originalsourceid><addsrcrecordid>eNqNkbFOwzAQhi0EEqXwBCyWWFhKfHbi2GMU0hIpTao2GZis4NoiqG1KnA68PYlaMaMb7nT69A__h9AjkBcgQniU-DATlAReGIIHXgbBFZpcvsCu_24S3KI7574IoYSDmKA4wq_vebRM4yjDm3SRR2W1TnAxx8sqK9NVluBNmWRZtMarYlVlUZkW-QanOfZDXFZxlEfJPbqx9c6Zh8ueomqelPHbLCsWY-5M-4Hfz6TR0lge0pDxLaecBEKCbwzIUFpafwQhDSy1mnFNhZVcSgNbzagNasu4lWyKns65resb5XTTG_2p28PB6F5RCiBCYAP1fKaOXft9Mq5X-8Zps9vVB9OenALOpRCcUv4f1KcwzoCyM6q71rnOWHXsmn3d_SgganSgxobV2LAaHChQgwP2C-uvcNQ</addsrcrecordid><sourcetype>Open Access Repository</sourcetype><iscdi>true</iscdi><recordtype>article</recordtype><pqid>1664212121</pqid></control><display><type>article</type><title>A DYNAMICAL SIGNATURE OF MULTIPLE STELLAR POPULATIONS IN 47 TUCANAE</title><source>EZB-FREE-00999 freely available EZB journals</source><creator>Richer, Harvey B ; Heyl, Jeremy ; Anderson, Jay ; Kalirai, Jason S ; Shara, Michael M ; Dotter, Aaron ; Fahlman, Gregory G ; Rich, R Michael</creator><creatorcontrib>Richer, Harvey B ; Heyl, Jeremy ; Anderson, Jay ; Kalirai, Jason S ; Shara, Michael M ; Dotter, Aaron ; Fahlman, Gregory G ; Rich, R Michael</creatorcontrib><description>Based on the width of its main sequence, and an actual observed split when viewed through particular filters, it is widely accepted that 47 Tucanae contains multiple stellar populations. In this contribution, we divide the main sequence of 47 Tuc into four color groups, which presumably represent stars of various chemical compositions. The kinematic properties of each of these groups are explored via proper motions, and a strong signal emerges of differing proper-motion anisotropies with differing main-sequence color; the bluest main-sequence stars exhibit the largest proper-motion anisotropy which becomes undetectable for the reddest stars. In addition, the bluest stars are also the most centrally concentrated. A similar analysis for Small Magellanic Cloud stars, which are located in the background of 47 Tuc on our frames, yields none of the anisotropy exhibited by the 47 Tuc stars. We discuss implications of these results for possible formation scenarios of the various populations.</description><identifier>ISSN: 2041-8205</identifier><identifier>EISSN: 2041-8213</identifier><identifier>DOI: 10.1088/2041-8205/771/1/L15</identifier><language>eng</language><publisher>United States</publisher><subject>ANISOTROPY ; ASTRONOMY ; ASTROPHYSICS ; ASTROPHYSICS, COSMOLOGY AND ASTRONOMY ; CHEMICAL COMPOSITION ; Color ; Frames ; HERTZSPRUNG-RUSSELL DIAGRAM ; Kinematics ; MAGELLANIC CLOUDS ; MAIN SEQUENCE STARS ; OPTICAL FILTERS ; PROPER MOTION ; RED GIANT STARS ; Signatures ; Stars ; Stellar populations</subject><ispartof>Astrophysical journal. Letters, 2013-07, Vol.771 (1), p.1-5</ispartof><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c454t-9ec9ef672736d626058914ee1979f2ab5725f2fc36c28f9699e1dc32f5af36f93</citedby><cites>FETCH-LOGICAL-c454t-9ec9ef672736d626058914ee1979f2ab5725f2fc36c28f9699e1dc32f5af36f93</cites></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/22118713$$D View this record in Osti.gov$$Hfree_for_read</backlink></links><search><creatorcontrib>Richer, Harvey B</creatorcontrib><creatorcontrib>Heyl, Jeremy</creatorcontrib><creatorcontrib>Anderson, Jay</creatorcontrib><creatorcontrib>Kalirai, Jason S</creatorcontrib><creatorcontrib>Shara, Michael M</creatorcontrib><creatorcontrib>Dotter, Aaron</creatorcontrib><creatorcontrib>Fahlman, Gregory G</creatorcontrib><creatorcontrib>Rich, R Michael</creatorcontrib><title>A DYNAMICAL SIGNATURE OF MULTIPLE STELLAR POPULATIONS IN 47 TUCANAE</title><title>Astrophysical journal. Letters</title><description>Based on the width of its main sequence, and an actual observed split when viewed through particular filters, it is widely accepted that 47 Tucanae contains multiple stellar populations. In this contribution, we divide the main sequence of 47 Tuc into four color groups, which presumably represent stars of various chemical compositions. The kinematic properties of each of these groups are explored via proper motions, and a strong signal emerges of differing proper-motion anisotropies with differing main-sequence color; the bluest main-sequence stars exhibit the largest proper-motion anisotropy which becomes undetectable for the reddest stars. In addition, the bluest stars are also the most centrally concentrated. A similar analysis for Small Magellanic Cloud stars, which are located in the background of 47 Tuc on our frames, yields none of the anisotropy exhibited by the 47 Tuc stars. We discuss implications of these results for possible formation scenarios of the various populations.</description><subject>ANISOTROPY</subject><subject>ASTRONOMY</subject><subject>ASTROPHYSICS</subject><subject>ASTROPHYSICS, COSMOLOGY AND ASTRONOMY</subject><subject>CHEMICAL COMPOSITION</subject><subject>Color</subject><subject>Frames</subject><subject>HERTZSPRUNG-RUSSELL DIAGRAM</subject><subject>Kinematics</subject><subject>MAGELLANIC CLOUDS</subject><subject>MAIN SEQUENCE STARS</subject><subject>OPTICAL FILTERS</subject><subject>PROPER MOTION</subject><subject>RED GIANT STARS</subject><subject>Signatures</subject><subject>Stars</subject><subject>Stellar populations</subject><issn>2041-8205</issn><issn>2041-8213</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2013</creationdate><recordtype>article</recordtype><recordid>eNqNkbFOwzAQhi0EEqXwBCyWWFhKfHbi2GMU0hIpTao2GZis4NoiqG1KnA68PYlaMaMb7nT69A__h9AjkBcgQniU-DATlAReGIIHXgbBFZpcvsCu_24S3KI7574IoYSDmKA4wq_vebRM4yjDm3SRR2W1TnAxx8sqK9NVluBNmWRZtMarYlVlUZkW-QanOfZDXFZxlEfJPbqx9c6Zh8ueomqelPHbLCsWY-5M-4Hfz6TR0lge0pDxLaecBEKCbwzIUFpafwQhDSy1mnFNhZVcSgNbzagNasu4lWyKns65resb5XTTG_2p28PB6F5RCiBCYAP1fKaOXft9Mq5X-8Zps9vVB9OenALOpRCcUv4f1KcwzoCyM6q71rnOWHXsmn3d_SgganSgxobV2LAaHChQgwP2C-uvcNQ</recordid><startdate>20130701</startdate><enddate>20130701</enddate><creator>Richer, Harvey B</creator><creator>Heyl, Jeremy</creator><creator>Anderson, Jay</creator><creator>Kalirai, Jason S</creator><creator>Shara, Michael M</creator><creator>Dotter, Aaron</creator><creator>Fahlman, Gregory G</creator><creator>Rich, R Michael</creator><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>KL.</scope><scope>8FD</scope><scope>H8D</scope><scope>L7M</scope><scope>OTOTI</scope></search><sort><creationdate>20130701</creationdate><title>A DYNAMICAL SIGNATURE OF MULTIPLE STELLAR POPULATIONS IN 47 TUCANAE</title><author>Richer, Harvey B ; Heyl, Jeremy ; Anderson, Jay ; Kalirai, Jason S ; Shara, Michael M ; Dotter, Aaron ; Fahlman, Gregory G ; Rich, R Michael</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c454t-9ec9ef672736d626058914ee1979f2ab5725f2fc36c28f9699e1dc32f5af36f93</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2013</creationdate><topic>ANISOTROPY</topic><topic>ASTRONOMY</topic><topic>ASTROPHYSICS</topic><topic>ASTROPHYSICS, COSMOLOGY AND ASTRONOMY</topic><topic>CHEMICAL COMPOSITION</topic><topic>Color</topic><topic>Frames</topic><topic>HERTZSPRUNG-RUSSELL DIAGRAM</topic><topic>Kinematics</topic><topic>MAGELLANIC CLOUDS</topic><topic>MAIN SEQUENCE STARS</topic><topic>OPTICAL FILTERS</topic><topic>PROPER MOTION</topic><topic>RED GIANT STARS</topic><topic>Signatures</topic><topic>Stars</topic><topic>Stellar populations</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Richer, Harvey B</creatorcontrib><creatorcontrib>Heyl, Jeremy</creatorcontrib><creatorcontrib>Anderson, Jay</creatorcontrib><creatorcontrib>Kalirai, Jason S</creatorcontrib><creatorcontrib>Shara, Michael M</creatorcontrib><creatorcontrib>Dotter, Aaron</creatorcontrib><creatorcontrib>Fahlman, Gregory G</creatorcontrib><creatorcontrib>Rich, R Michael</creatorcontrib><collection>CrossRef</collection><collection>Meteorological &amp; Geoastrophysical Abstracts</collection><collection>Meteorological &amp; Geoastrophysical Abstracts - Academic</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>OSTI.GOV</collection><jtitle>Astrophysical journal. Letters</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Richer, Harvey B</au><au>Heyl, Jeremy</au><au>Anderson, Jay</au><au>Kalirai, Jason S</au><au>Shara, Michael M</au><au>Dotter, Aaron</au><au>Fahlman, Gregory G</au><au>Rich, R Michael</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>A DYNAMICAL SIGNATURE OF MULTIPLE STELLAR POPULATIONS IN 47 TUCANAE</atitle><jtitle>Astrophysical journal. Letters</jtitle><date>2013-07-01</date><risdate>2013</risdate><volume>771</volume><issue>1</issue><spage>1</spage><epage>5</epage><pages>1-5</pages><issn>2041-8205</issn><eissn>2041-8213</eissn><abstract>Based on the width of its main sequence, and an actual observed split when viewed through particular filters, it is widely accepted that 47 Tucanae contains multiple stellar populations. In this contribution, we divide the main sequence of 47 Tuc into four color groups, which presumably represent stars of various chemical compositions. The kinematic properties of each of these groups are explored via proper motions, and a strong signal emerges of differing proper-motion anisotropies with differing main-sequence color; the bluest main-sequence stars exhibit the largest proper-motion anisotropy which becomes undetectable for the reddest stars. In addition, the bluest stars are also the most centrally concentrated. A similar analysis for Small Magellanic Cloud stars, which are located in the background of 47 Tuc on our frames, yields none of the anisotropy exhibited by the 47 Tuc stars. We discuss implications of these results for possible formation scenarios of the various populations.</abstract><cop>United States</cop><doi>10.1088/2041-8205/771/1/L15</doi><tpages>5</tpages><oa>free_for_read</oa></addata></record>
fulltext fulltext
identifier ISSN: 2041-8205
ispartof Astrophysical journal. Letters, 2013-07, Vol.771 (1), p.1-5
issn 2041-8205
2041-8213
language eng
recordid cdi_osti_scitechconnect_22118713
source EZB-FREE-00999 freely available EZB journals
subjects ANISOTROPY
ASTRONOMY
ASTROPHYSICS
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
CHEMICAL COMPOSITION
Color
Frames
HERTZSPRUNG-RUSSELL DIAGRAM
Kinematics
MAGELLANIC CLOUDS
MAIN SEQUENCE STARS
OPTICAL FILTERS
PROPER MOTION
RED GIANT STARS
Signatures
Stars
Stellar populations
title A DYNAMICAL SIGNATURE OF MULTIPLE STELLAR POPULATIONS IN 47 TUCANAE
url http://sfxeu10.hosted.exlibrisgroup.com/loughborough?ctx_ver=Z39.88-2004&ctx_enc=info:ofi/enc:UTF-8&ctx_tim=2024-12-26T20%3A25%3A54IST&url_ver=Z39.88-2004&url_ctx_fmt=infofi/fmt:kev:mtx:ctx&rfr_id=info:sid/primo.exlibrisgroup.com:primo3-Article-proquest_osti_&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.genre=article&rft.atitle=A%20DYNAMICAL%20SIGNATURE%20OF%20MULTIPLE%20STELLAR%20POPULATIONS%20IN%2047%20TUCANAE&rft.jtitle=Astrophysical%20journal.%20Letters&rft.au=Richer,%20Harvey%20B&rft.date=2013-07-01&rft.volume=771&rft.issue=1&rft.spage=1&rft.epage=5&rft.pages=1-5&rft.issn=2041-8205&rft.eissn=2041-8213&rft_id=info:doi/10.1088/2041-8205/771/1/L15&rft_dat=%3Cproquest_osti_%3E1669886226%3C/proquest_osti_%3E%3Cgrp_id%3Ecdi_FETCH-LOGICAL-c454t-9ec9ef672736d626058914ee1979f2ab5725f2fc36c28f9699e1dc32f5af36f93%3C/grp_id%3E%3Coa%3E%3C/oa%3E%3Curl%3E%3C/url%3E&rft_id=info:oai/&rft_pqid=1664212121&rft_id=info:pmid/&rfr_iscdi=true