Beyond the Local Volume. II. Population Scaleheights and Ages of Ultracool Dwarfs in Deep HST/WFC3 Parallel Fields
Ultracool dwarfs represent a significant proportion of stars in the Milky Way,and deep samples of these sources have the potential to constrain the formation history and evolution of low-mass objects in the Galaxy. Until recently, spectral samples have been limited to the local volume (d
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| creator | Aganze, Christian Burgasser, Adam J Malkan, Matthew A Theissen, Christopher A Tejada Arevalo, Roberto A Hsu, Chih-Chun Daniella C Bardalez Gagliuffi Ryan, Russell E Holwerda, Benne W |
| description | Ultracool dwarfs represent a significant proportion of stars in the Milky Way,and deep samples of these sources have the potential to constrain the formation history and evolution of low-mass objects in the Galaxy. Until recently, spectral samples have been limited to the local volume (d |
| doi_str_mv | 10.48550/arxiv.2204.07621 |
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Population Scaleheights and Ages of Ultracool Dwarfs in Deep HST/WFC3 Parallel Fields</title><source>arXiv.org</source><source>Free E- Journals</source><creator>Aganze, Christian ; Burgasser, Adam J ; Malkan, Matthew A ; Theissen, Christopher A ; Tejada Arevalo, Roberto A ; Hsu, Chih-Chun ; Daniella C Bardalez Gagliuffi ; Ryan, Russell E ; Holwerda, Benne W</creator><creatorcontrib>Aganze, Christian ; Burgasser, Adam J ; Malkan, Matthew A ; Theissen, Christopher A ; Tejada Arevalo, Roberto A ; Hsu, Chih-Chun ; Daniella C Bardalez Gagliuffi ; Ryan, Russell E ; Holwerda, Benne W</creatorcontrib><description>Ultracool dwarfs represent a significant proportion of stars in the Milky Way,and deep samples of these sources have the potential to constrain the formation history and evolution of low-mass objects in the Galaxy. Until recently, spectral samples have been limited to the local volume (d<100 pc). Here, we analyze a sample of 164 spectroscopically-characterized ultracool dwarfs identified by Aganze et al. (2022) in the Hubble Space Telescope WFC3 Infrared Spectroscopic Parallel (WISP) Survey and 3D-HST. We model the observed luminosity function using population simulations to place constraints on scaleheights, vertical velocity dispersions and population ages as a function of spectral type. Our star counts are consistent with a power-law mass function and constant star formation history for ultracool dwarfs, with vertical scaleheights 249\(_{-61}^{+48}\) pc for late M dwarfs, 153\(_{-30}^{+56}\) pc for L dwarfs, and 175\(_{-56}^{+149}\) pc for T dwarfs. Using spatial and velocity dispersion relations, these scaleheights correspond to disk population ages of 3.6\(_{-1.0}^{+0.8}\) for late M dwarfs, 2.1\(_{-0.5}^{+0.9}\) Gyr for L dwarfs, and 2.4\(_{-0.8}^{+2.4}\) Gyr for T dwarfs, which are consistent with prior simulations that predict that L-type dwarfs are on average a younger and less dispersed population. There is an additional 1-2 Gyr systematic uncertainty on these ages due to variances in age-velocity relations. We use our population simulations to predict the UCD yield in the JWST PASSAGES survey, a similar and deeper survey to WISPS and 3D-HST, and find that it will produce a comparably-sized UCD sample, albeit dominated by thick disk and halo sources.</description><identifier>EISSN: 2331-8422</identifier><identifier>DOI: 10.48550/arxiv.2204.07621</identifier><language>eng</language><publisher>Ithaca: Cornell University Library, arXiv.org</publisher><subject>Age ; Constraint modelling ; Hubble Space Telescope ; Infrared spectroscopy ; Infrared telescopes ; Luminosity ; Physics - Astrophysics of Galaxies ; Physics - Solar and Stellar Astrophysics ; Population ; Red dwarf stars ; Simulation ; Space telescopes ; Star & galaxy formation ; Star formation ; Three dimensional models</subject><ispartof>arXiv.org, 2022-08</ispartof><rights>2022. 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>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>228,230,776,780,881,27902</link.rule.ids><backlink>$$Uhttps://doi.org/10.48550/arXiv.2204.07621$$DView paper in arXiv$$Hfree_for_read</backlink><backlink>$$Uhttps://doi.org/10.3847/1538-4357/ac7053$$DView published paper (Access to full text may be restricted)$$Hfree_for_read</backlink></links><search><creatorcontrib>Aganze, Christian</creatorcontrib><creatorcontrib>Burgasser, Adam J</creatorcontrib><creatorcontrib>Malkan, Matthew A</creatorcontrib><creatorcontrib>Theissen, Christopher A</creatorcontrib><creatorcontrib>Tejada Arevalo, Roberto A</creatorcontrib><creatorcontrib>Hsu, Chih-Chun</creatorcontrib><creatorcontrib>Daniella C Bardalez Gagliuffi</creatorcontrib><creatorcontrib>Ryan, Russell E</creatorcontrib><creatorcontrib>Holwerda, Benne W</creatorcontrib><title>Beyond the Local Volume. II. Population Scaleheights and Ages of Ultracool Dwarfs in Deep HST/WFC3 Parallel Fields</title><title>arXiv.org</title><description>Ultracool dwarfs represent a significant proportion of stars in the Milky Way,and deep samples of these sources have the potential to constrain the formation history and evolution of low-mass objects in the Galaxy. Until recently, spectral samples have been limited to the local volume (d<100 pc). Here, we analyze a sample of 164 spectroscopically-characterized ultracool dwarfs identified by Aganze et al. (2022) in the Hubble Space Telescope WFC3 Infrared Spectroscopic Parallel (WISP) Survey and 3D-HST. We model the observed luminosity function using population simulations to place constraints on scaleheights, vertical velocity dispersions and population ages as a function of spectral type. Our star counts are consistent with a power-law mass function and constant star formation history for ultracool dwarfs, with vertical scaleheights 249\(_{-61}^{+48}\) pc for late M dwarfs, 153\(_{-30}^{+56}\) pc for L dwarfs, and 175\(_{-56}^{+149}\) pc for T dwarfs. Using spatial and velocity dispersion relations, these scaleheights correspond to disk population ages of 3.6\(_{-1.0}^{+0.8}\) for late M dwarfs, 2.1\(_{-0.5}^{+0.9}\) Gyr for L dwarfs, and 2.4\(_{-0.8}^{+2.4}\) Gyr for T dwarfs, which are consistent with prior simulations that predict that L-type dwarfs are on average a younger and less dispersed population. There is an additional 1-2 Gyr systematic uncertainty on these ages due to variances in age-velocity relations. We use our population simulations to predict the UCD yield in the JWST PASSAGES survey, a similar and deeper survey to WISPS and 3D-HST, and find that it will produce a comparably-sized UCD sample, albeit dominated by thick disk and halo sources.</description><subject>Age</subject><subject>Constraint modelling</subject><subject>Hubble Space Telescope</subject><subject>Infrared spectroscopy</subject><subject>Infrared telescopes</subject><subject>Luminosity</subject><subject>Physics - Astrophysics of Galaxies</subject><subject>Physics - Solar and Stellar Astrophysics</subject><subject>Population</subject><subject>Red dwarf stars</subject><subject>Simulation</subject><subject>Space telescopes</subject><subject>Star & galaxy formation</subject><subject>Star formation</subject><subject>Three dimensional models</subject><issn>2331-8422</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2022</creationdate><recordtype>article</recordtype><sourceid>BENPR</sourceid><sourceid>GOX</sourceid><recordid>eNotkE9PwkAQxTcmJhLkA3hyEs8t-5_tEUGEhEQSUI_Ntt1CydLF3Vbl21vA08u8eTN5-SH0QHDMlRB4qP1v9R1TinmMR5KSG9SjjJFIcUrv0CCEPcaYyhEVgvWQfzYnVxfQ7AwsXa4tfDjbHkwMi0UMK3dsrW4qV8O625mdqba7JoDuLsZbE8CV8G4br3PnLEx_tC8DVDVMjTnCfL0Zfs4mDFbaa2uNhVllbBHu0W2pbTCDf-2jzexlM5lHy7fXxWS8jLSgMspKRQnNGGFFRnKuOqEJV92oSaazjJ99TnLCMqVE0nkyEVIkBWdCiFyyPnq8vr0ASY--Omh_Ss9g0guYLvF0TRy9-2pNaNK9a33ddUqpFHREFceS_QHadWP2</recordid><startdate>20220817</startdate><enddate>20220817</enddate><creator>Aganze, Christian</creator><creator>Burgasser, Adam J</creator><creator>Malkan, Matthew A</creator><creator>Theissen, Christopher A</creator><creator>Tejada Arevalo, Roberto A</creator><creator>Hsu, Chih-Chun</creator><creator>Daniella C Bardalez Gagliuffi</creator><creator>Ryan, Russell E</creator><creator>Holwerda, Benne W</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>20220817</creationdate><title>Beyond the Local Volume. 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Population Scaleheights and Ages of Ultracool Dwarfs in Deep HST/WFC3 Parallel Fields</title><author>Aganze, Christian ; Burgasser, Adam J ; Malkan, Matthew A ; Theissen, Christopher A ; Tejada Arevalo, Roberto A ; Hsu, Chih-Chun ; Daniella C Bardalez Gagliuffi ; Ryan, Russell E ; Holwerda, Benne W</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-a526-bf8212b313db1c483db294813da1babb43db141c13b88591ba695659d43555c63</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2022</creationdate><topic>Age</topic><topic>Constraint modelling</topic><topic>Hubble Space Telescope</topic><topic>Infrared spectroscopy</topic><topic>Infrared telescopes</topic><topic>Luminosity</topic><topic>Physics - Astrophysics of Galaxies</topic><topic>Physics - Solar and Stellar Astrophysics</topic><topic>Population</topic><topic>Red dwarf stars</topic><topic>Simulation</topic><topic>Space telescopes</topic><topic>Star & galaxy formation</topic><topic>Star formation</topic><topic>Three dimensional models</topic><toplevel>online_resources</toplevel><creatorcontrib>Aganze, Christian</creatorcontrib><creatorcontrib>Burgasser, Adam J</creatorcontrib><creatorcontrib>Malkan, Matthew A</creatorcontrib><creatorcontrib>Theissen, Christopher A</creatorcontrib><creatorcontrib>Tejada Arevalo, Roberto A</creatorcontrib><creatorcontrib>Hsu, Chih-Chun</creatorcontrib><creatorcontrib>Daniella C Bardalez Gagliuffi</creatorcontrib><creatorcontrib>Ryan, Russell E</creatorcontrib><creatorcontrib>Holwerda, Benne W</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>Aganze, Christian</au><au>Burgasser, Adam J</au><au>Malkan, Matthew A</au><au>Theissen, Christopher A</au><au>Tejada Arevalo, Roberto A</au><au>Hsu, Chih-Chun</au><au>Daniella C Bardalez Gagliuffi</au><au>Ryan, Russell E</au><au>Holwerda, Benne W</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Beyond the Local Volume. II. Population Scaleheights and Ages of Ultracool Dwarfs in Deep HST/WFC3 Parallel Fields</atitle><jtitle>arXiv.org</jtitle><date>2022-08-17</date><risdate>2022</risdate><eissn>2331-8422</eissn><abstract>Ultracool dwarfs represent a significant proportion of stars in the Milky Way,and deep samples of these sources have the potential to constrain the formation history and evolution of low-mass objects in the Galaxy. Until recently, spectral samples have been limited to the local volume (d<100 pc). Here, we analyze a sample of 164 spectroscopically-characterized ultracool dwarfs identified by Aganze et al. (2022) in the Hubble Space Telescope WFC3 Infrared Spectroscopic Parallel (WISP) Survey and 3D-HST. We model the observed luminosity function using population simulations to place constraints on scaleheights, vertical velocity dispersions and population ages as a function of spectral type. Our star counts are consistent with a power-law mass function and constant star formation history for ultracool dwarfs, with vertical scaleheights 249\(_{-61}^{+48}\) pc for late M dwarfs, 153\(_{-30}^{+56}\) pc for L dwarfs, and 175\(_{-56}^{+149}\) pc for T dwarfs. Using spatial and velocity dispersion relations, these scaleheights correspond to disk population ages of 3.6\(_{-1.0}^{+0.8}\) for late M dwarfs, 2.1\(_{-0.5}^{+0.9}\) Gyr for L dwarfs, and 2.4\(_{-0.8}^{+2.4}\) Gyr for T dwarfs, which are consistent with prior simulations that predict that L-type dwarfs are on average a younger and less dispersed population. There is an additional 1-2 Gyr systematic uncertainty on these ages due to variances in age-velocity relations. We use our population simulations to predict the UCD yield in the JWST PASSAGES survey, a similar and deeper survey to WISPS and 3D-HST, and find that it will produce a comparably-sized UCD sample, albeit dominated by thick disk and halo sources.</abstract><cop>Ithaca</cop><pub>Cornell University Library, arXiv.org</pub><doi>10.48550/arxiv.2204.07621</doi><oa>free_for_read</oa></addata></record> |
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| subjects | Age Constraint modelling Hubble Space Telescope Infrared spectroscopy Infrared telescopes Luminosity Physics - Astrophysics of Galaxies Physics - Solar and Stellar Astrophysics Population Red dwarf stars Simulation Space telescopes Star & galaxy formation Star formation Three dimensional models |
| title | Beyond the Local Volume. II. Population Scaleheights and Ages of Ultracool Dwarfs in Deep HST/WFC3 Parallel Fields |
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