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Vertical Phase Mixing across the Galactic Disk
By combining the Large Sky Area Multi-object Fiber Spectroscopic Telescope and Gaia data, we investigate the vertical phase mixing across the Galactic disk. Our results confirm the existence of phase space snail shells (or phase spirals) from 6–12 kpc. We find that grouping stars by the guiding radi...
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Published in: | The Astrophysical journal 2021-04, Vol.911 (2), p.107 |
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description | By combining the Large Sky Area Multi-object Fiber Spectroscopic Telescope and Gaia data, we investigate the vertical phase mixing across the Galactic disk. Our results confirm the existence of phase space snail shells (or phase spirals) from 6–12 kpc. We find that grouping stars by the guiding radius (
R
g
), instead of the present radius (
R
), further enhances the snail shell signal in the following aspects: (1) clarity of the snail shell shape is increased; (2) more wraps of the snail shell can be seen; (3) the phase spaces are less affected by the lack of stars closer to the disk midplane due to extinction; and (4) the phase space snail shell is amplified in greater radial ranges. Compared to the
R
-based snail shell, the quantitatively measured shapes are similar, except that the
R
g
-based snail shells show more wraps with a better contrast. These lines of evidence lead to the conclusion that the guiding radius (angular momentum) is a fundamental parameter tracing the phase space snail shell across the Galactic disk. Results of our test particle simulations with impulse approximation verify that particles grouped according to
R
g
reveal well-defined and sharper snail shell features. By comparing the radial profiles of the snail shell pitch angle between the observation and simulation, the external perturbation can be constrained to ∼500−700 Myr ago. For future vertical phase mixing study, it is recommended to use the guiding radius with additional constraints on orbital hotness (ellipticity) to improve the clarity of the phase snail. |
doi_str_mv | 10.3847/1538-4357/abea17 |
format | article |
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R
g
), instead of the present radius (
R
), further enhances the snail shell signal in the following aspects: (1) clarity of the snail shell shape is increased; (2) more wraps of the snail shell can be seen; (3) the phase spaces are less affected by the lack of stars closer to the disk midplane due to extinction; and (4) the phase space snail shell is amplified in greater radial ranges. Compared to the
R
-based snail shell, the quantitatively measured shapes are similar, except that the
R
g
-based snail shells show more wraps with a better contrast. These lines of evidence lead to the conclusion that the guiding radius (angular momentum) is a fundamental parameter tracing the phase space snail shell across the Galactic disk. Results of our test particle simulations with impulse approximation verify that particles grouped according to
R
g
reveal well-defined and sharper snail shell features. By comparing the radial profiles of the snail shell pitch angle between the observation and simulation, the external perturbation can be constrained to ∼500−700 Myr ago. For future vertical phase mixing study, it is recommended to use the guiding radius with additional constraints on orbital hotness (ellipticity) to improve the clarity of the phase snail.</description><identifier>ISSN: 0004-637X</identifier><identifier>EISSN: 1538-4357</identifier><identifier>DOI: 10.3847/1538-4357/abea17</identifier><language>eng</language><publisher>Philadelphia: The American Astronomical Society</publisher><subject>Angular momentum ; Astrophysics ; Clarity ; Constraints ; Ellipticity ; Galactic disk ; Milky Way disk ; Milky Way dynamics ; Milky Way evolution ; Milky Way Galaxy ; Perturbation ; Pitch (inclination) ; Spectroscopic telescopes ; Spirals</subject><ispartof>The Astrophysical journal, 2021-04, Vol.911 (2), p.107</ispartof><rights>2021. The Author(s). Published by the American Astronomical Society.</rights><rights>Copyright IOP Publishing Apr 01, 2021</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c380t-eb43a67f79cc2c95e5c483c6ad4f03eb5ea895096356a669187642f23ba8af813</citedby><cites>FETCH-LOGICAL-c380t-eb43a67f79cc2c95e5c483c6ad4f03eb5ea895096356a669187642f23ba8af813</cites><orcidid>0000-0001-5017-7021</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail></links><search><creatorcontrib>Li, Zhao-Yu</creatorcontrib><title>Vertical Phase Mixing across the Galactic Disk</title><title>The Astrophysical journal</title><addtitle>APJ</addtitle><addtitle>Astrophys. J</addtitle><description>By combining the Large Sky Area Multi-object Fiber Spectroscopic Telescope and Gaia data, we investigate the vertical phase mixing across the Galactic disk. Our results confirm the existence of phase space snail shells (or phase spirals) from 6–12 kpc. We find that grouping stars by the guiding radius (
R
g
), instead of the present radius (
R
), further enhances the snail shell signal in the following aspects: (1) clarity of the snail shell shape is increased; (2) more wraps of the snail shell can be seen; (3) the phase spaces are less affected by the lack of stars closer to the disk midplane due to extinction; and (4) the phase space snail shell is amplified in greater radial ranges. Compared to the
R
-based snail shell, the quantitatively measured shapes are similar, except that the
R
g
-based snail shells show more wraps with a better contrast. These lines of evidence lead to the conclusion that the guiding radius (angular momentum) is a fundamental parameter tracing the phase space snail shell across the Galactic disk. Results of our test particle simulations with impulse approximation verify that particles grouped according to
R
g
reveal well-defined and sharper snail shell features. By comparing the radial profiles of the snail shell pitch angle between the observation and simulation, the external perturbation can be constrained to ∼500−700 Myr ago. For future vertical phase mixing study, it is recommended to use the guiding radius with additional constraints on orbital hotness (ellipticity) to improve the clarity of the phase snail.</description><subject>Angular momentum</subject><subject>Astrophysics</subject><subject>Clarity</subject><subject>Constraints</subject><subject>Ellipticity</subject><subject>Galactic disk</subject><subject>Milky Way disk</subject><subject>Milky Way dynamics</subject><subject>Milky Way evolution</subject><subject>Milky Way Galaxy</subject><subject>Perturbation</subject><subject>Pitch (inclination)</subject><subject>Spectroscopic telescopes</subject><subject>Spirals</subject><issn>0004-637X</issn><issn>1538-4357</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2021</creationdate><recordtype>article</recordtype><recordid>eNp9kE1Lw0AQhhdRMFbvHgPizbS72e-j1FqFih5UvC2T7a5NrE3cTUH_vYkRvYinYYbnnRkehI4JHlPF5IRwqjJGuZxA4YDIHZT8jHZRgjFmmaDyaR8dxFj1ba51gsaPLrSlhXV6t4Lo0pvyvdw8p2BDHWParlw6hzXYDkkvyvhyiPY8rKM7-q4j9HA5u59eZYvb-fX0fJFZqnCbuYJRENJLbW1uNXfcMkWtgCXzmLqCO1CaYy0oFyCEJkoKlvucFqDAK0JH6GTY24T6betia6p6GzbdSZPzjpaYCdFReKC-vg3OmyaUrxA-DMGmt2J6BaZXYAYrXeRsiJR187vzH_z0DxyaymhCTN4FpWmWnn4CellufA</recordid><startdate>20210401</startdate><enddate>20210401</enddate><creator>Li, Zhao-Yu</creator><general>The American Astronomical Society</general><general>IOP Publishing</general><scope>O3W</scope><scope>TSCCA</scope><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/0000-0001-5017-7021</orcidid></search><sort><creationdate>20210401</creationdate><title>Vertical Phase Mixing across the Galactic Disk</title><author>Li, Zhao-Yu</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c380t-eb43a67f79cc2c95e5c483c6ad4f03eb5ea895096356a669187642f23ba8af813</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2021</creationdate><topic>Angular momentum</topic><topic>Astrophysics</topic><topic>Clarity</topic><topic>Constraints</topic><topic>Ellipticity</topic><topic>Galactic disk</topic><topic>Milky Way disk</topic><topic>Milky Way dynamics</topic><topic>Milky Way evolution</topic><topic>Milky Way Galaxy</topic><topic>Perturbation</topic><topic>Pitch (inclination)</topic><topic>Spectroscopic telescopes</topic><topic>Spirals</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Li, Zhao-Yu</creatorcontrib><collection>IOP Publishing Free Content</collection><collection>IOPscience (Open Access)</collection><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>The Astrophysical journal</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Li, Zhao-Yu</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Vertical Phase Mixing across the Galactic Disk</atitle><jtitle>The Astrophysical journal</jtitle><stitle>APJ</stitle><addtitle>Astrophys. J</addtitle><date>2021-04-01</date><risdate>2021</risdate><volume>911</volume><issue>2</issue><spage>107</spage><pages>107-</pages><issn>0004-637X</issn><eissn>1538-4357</eissn><abstract>By combining the Large Sky Area Multi-object Fiber Spectroscopic Telescope and Gaia data, we investigate the vertical phase mixing across the Galactic disk. Our results confirm the existence of phase space snail shells (or phase spirals) from 6–12 kpc. We find that grouping stars by the guiding radius (
R
g
), instead of the present radius (
R
), further enhances the snail shell signal in the following aspects: (1) clarity of the snail shell shape is increased; (2) more wraps of the snail shell can be seen; (3) the phase spaces are less affected by the lack of stars closer to the disk midplane due to extinction; and (4) the phase space snail shell is amplified in greater radial ranges. Compared to the
R
-based snail shell, the quantitatively measured shapes are similar, except that the
R
g
-based snail shells show more wraps with a better contrast. These lines of evidence lead to the conclusion that the guiding radius (angular momentum) is a fundamental parameter tracing the phase space snail shell across the Galactic disk. Results of our test particle simulations with impulse approximation verify that particles grouped according to
R
g
reveal well-defined and sharper snail shell features. By comparing the radial profiles of the snail shell pitch angle between the observation and simulation, the external perturbation can be constrained to ∼500−700 Myr ago. For future vertical phase mixing study, it is recommended to use the guiding radius with additional constraints on orbital hotness (ellipticity) to improve the clarity of the phase snail.</abstract><cop>Philadelphia</cop><pub>The American Astronomical Society</pub><doi>10.3847/1538-4357/abea17</doi><tpages>27</tpages><orcidid>https://orcid.org/0000-0001-5017-7021</orcidid><oa>free_for_read</oa></addata></record> |
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source | In der EZB frei verfügbare Zeitschriften |
subjects | Angular momentum Astrophysics Clarity Constraints Ellipticity Galactic disk Milky Way disk Milky Way dynamics Milky Way evolution Milky Way Galaxy Perturbation Pitch (inclination) Spectroscopic telescopes Spirals |
title | Vertical Phase Mixing across the Galactic Disk |
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