On the Significance of the Thick Disks of Disk Galaxies
Thick disks are a prevalent feature observed in numerous disk galaxies, including our own Milky Way. Their significance has been reported to vary widely, ranging from a few percent to 100% of the disk mass, depending on the galaxy and the measurement method. We use the NewHorizon simulation, which h...
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| Veröffentlicht in: | The Astrophysical Journal Supplement Series 2024-03, Vol.271 (1), p.1 |
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| creator | Yi, Sukyoung K. Jang, J. K. Devriendt, Julien Dubois, Yohan Han, San Kimm, Taysun Kraljic, Katarina Park, Minjung Peirani, Sebastien Pichon, Christophe Rhee, Jinsu |
| description | Thick disks are a prevalent feature observed in numerous disk galaxies, including our own Milky Way. Their significance has been reported to vary widely, ranging from a few percent to 100% of the disk mass, depending on the galaxy and the measurement method. We use the NewHorizon simulation, which has high spatial and stellar mass resolutions, to investigate the issue of the thick-disk mass fraction. We also use the NewHorizon2 simulation, which was run on the same initial conditions, but additionally traced nine chemical elements. Based on a sample of 27 massive disk galaxies with
M
*
> 10
10
M
⊙
in NewHorizon, the contribution of the thick disk was found to be 20% ± 11% in
r
-band luminosity or 35% ± 15% in mass to the overall galactic disk, which seems in agreement with observational data. The vertical profiles of 0, 22, and 5 galaxies are best fitted by 1, 2, or 3
sech
2
components, respectively. The NewHorizon2 data show that the selection of thick-disk stars based on a single [
α
/Fe] cut is contaminated by stars of different kinematic properties, while missing the bulk of kinematically thick disk stars. Vertical luminosity profile fits recover the key properties of thick disks reasonably well. The majority of stars are born near the galactic midplane with high circularity and get heated with time via fluctuations in the force field. Depending on the star formation and merger histories, galaxies may naturally develop thick disks with significantly different properties. |
| doi_str_mv | 10.3847/1538-4365/ad0e71 |
| format | Article |
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M
*
> 10
10
M
⊙
in NewHorizon, the contribution of the thick disk was found to be 20% ± 11% in
r
-band luminosity or 35% ± 15% in mass to the overall galactic disk, which seems in agreement with observational data. The vertical profiles of 0, 22, and 5 galaxies are best fitted by 1, 2, or 3
sech
2
components, respectively. The NewHorizon2 data show that the selection of thick-disk stars based on a single [
α
/Fe] cut is contaminated by stars of different kinematic properties, while missing the bulk of kinematically thick disk stars. Vertical luminosity profile fits recover the key properties of thick disks reasonably well. The majority of stars are born near the galactic midplane with high circularity and get heated with time via fluctuations in the force field. Depending on the star formation and merger histories, galaxies may naturally develop thick disks with significantly different properties.</description><identifier>ISSN: 0067-0049</identifier><identifier>EISSN: 1538-4365</identifier><identifier>DOI: 10.3847/1538-4365/ad0e71</identifier><language>eng</language><publisher>Saskatoon: The American Astronomical Society</publisher><subject>Chemical elements ; Disk galaxies ; Galactic disk ; Galaxies ; Galaxy chemical evolution ; Galaxy disks ; Galaxy stellar disks ; Galaxy structure ; Hydrodynamical simulations ; Initial conditions ; Kinematics ; Luminosity ; Measurement methods ; Milky Way ; Sciences of the Universe ; Star & galaxy formation ; Star formation ; Stars ; Stars & galaxies ; Stellar mass</subject><ispartof>The Astrophysical Journal Supplement Series, 2024-03, Vol.271 (1), p.1</ispartof><rights>2024. The Author(s). Published by the American Astronomical Society.</rights><rights>2024. The Author(s). Published by the American Astronomical Society. 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>Distributed under a Creative Commons Attribution 4.0 International License</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c480t-da052d2453d3e6dae20ad307a1db69d852eae8f4e20b319fbcdc98a39f26f0fc3</citedby><cites>FETCH-LOGICAL-c480t-da052d2453d3e6dae20ad307a1db69d852eae8f4e20b319fbcdc98a39f26f0fc3</cites><orcidid>0000-0003-0695-6735 ; 0000-0002-4556-2619 ; 0000-0002-3950-3997 ; 0000-0002-8435-9402 ; 0000-0002-8140-0422 ; 0000-0002-0184-9589 ; 0000-0002-0858-5264 ; 0000-0001-9939-713X ; 0000-0003-0225-6387 ; 0000-0001-6180-0245</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://iopscience.iop.org/article/10.3847/1538-4365/ad0e71/pdf$$EPDF$$P50$$Giop$$Hfree_for_read</linktopdf><link.rule.ids>230,314,780,784,864,885,2100,27923,27924,38889,53866</link.rule.ids><backlink>$$Uhttps://insu.hal.science/insu-04490419$$DView record in HAL$$Hfree_for_read</backlink></links><search><creatorcontrib>Yi, Sukyoung K.</creatorcontrib><creatorcontrib>Jang, J. K.</creatorcontrib><creatorcontrib>Devriendt, Julien</creatorcontrib><creatorcontrib>Dubois, Yohan</creatorcontrib><creatorcontrib>Han, San</creatorcontrib><creatorcontrib>Kimm, Taysun</creatorcontrib><creatorcontrib>Kraljic, Katarina</creatorcontrib><creatorcontrib>Park, Minjung</creatorcontrib><creatorcontrib>Peirani, Sebastien</creatorcontrib><creatorcontrib>Pichon, Christophe</creatorcontrib><creatorcontrib>Rhee, Jinsu</creatorcontrib><title>On the Significance of the Thick Disks of Disk Galaxies</title><title>The Astrophysical Journal Supplement Series</title><addtitle>APJS</addtitle><addtitle>Astrophys. J. Suppl</addtitle><description>Thick disks are a prevalent feature observed in numerous disk galaxies, including our own Milky Way. Their significance has been reported to vary widely, ranging from a few percent to 100% of the disk mass, depending on the galaxy and the measurement method. We use the NewHorizon simulation, which has high spatial and stellar mass resolutions, to investigate the issue of the thick-disk mass fraction. We also use the NewHorizon2 simulation, which was run on the same initial conditions, but additionally traced nine chemical elements. Based on a sample of 27 massive disk galaxies with
M
*
> 10
10
M
⊙
in NewHorizon, the contribution of the thick disk was found to be 20% ± 11% in
r
-band luminosity or 35% ± 15% in mass to the overall galactic disk, which seems in agreement with observational data. The vertical profiles of 0, 22, and 5 galaxies are best fitted by 1, 2, or 3
sech
2
components, respectively. The NewHorizon2 data show that the selection of thick-disk stars based on a single [
α
/Fe] cut is contaminated by stars of different kinematic properties, while missing the bulk of kinematically thick disk stars. Vertical luminosity profile fits recover the key properties of thick disks reasonably well. The majority of stars are born near the galactic midplane with high circularity and get heated with time via fluctuations in the force field. Depending on the star formation and merger histories, galaxies may naturally develop thick disks with significantly different properties.</description><subject>Chemical elements</subject><subject>Disk galaxies</subject><subject>Galactic disk</subject><subject>Galaxies</subject><subject>Galaxy chemical evolution</subject><subject>Galaxy disks</subject><subject>Galaxy stellar disks</subject><subject>Galaxy structure</subject><subject>Hydrodynamical simulations</subject><subject>Initial conditions</subject><subject>Kinematics</subject><subject>Luminosity</subject><subject>Measurement methods</subject><subject>Milky Way</subject><subject>Sciences of the Universe</subject><subject>Star & galaxy formation</subject><subject>Star formation</subject><subject>Stars</subject><subject>Stars & galaxies</subject><subject>Stellar mass</subject><issn>0067-0049</issn><issn>1538-4365</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2024</creationdate><recordtype>article</recordtype><sourceid>O3W</sourceid><sourceid>DOA</sourceid><recordid>eNp9kUtLxDAURoMoOD72Lgu6Eqs3TdI0SxkfIwzMQl2H2zxmMo5tbWZE_72tFUUQySLh49zDDR8hRxTOWcHlBRWsSDnLxQVacJJukdF3tE1GALlMAbjaJXsxLgFACqZGRM6qZL1wyX2YV8EHg5VxSe0_s4dFME_JVYhPsY_6R3KLK3wLLh6QHY-r6A6_7n3yeHP9MJ6k09nt3fhymhpewDq1CCKzGRfMMpdbdBmgZSCR2jJXthCZQ1d43uUlo8qXxhpVIFM-yz14w_bJ3eC1NS5104ZnbN91jUF_BnU719iug1k5rUSucumxRMi58qwUxmcqc8a4UqB0net0cC1w9Us1uZzqUMWNBs4VcKpeaQcfD3DT1i8bF9d6WW_aqvur7qRCFFyxrKNgoExbx9g6_-2loPtedF-C7kvQQy_dyNkwEurmx_kPfvIHjs2y20NS3Z_GevYBfEOZOQ</recordid><startdate>20240301</startdate><enddate>20240301</enddate><creator>Yi, Sukyoung K.</creator><creator>Jang, J. 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K.</au><au>Devriendt, Julien</au><au>Dubois, Yohan</au><au>Han, San</au><au>Kimm, Taysun</au><au>Kraljic, Katarina</au><au>Park, Minjung</au><au>Peirani, Sebastien</au><au>Pichon, Christophe</au><au>Rhee, Jinsu</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>On the Significance of the Thick Disks of Disk Galaxies</atitle><jtitle>The Astrophysical Journal Supplement Series</jtitle><stitle>APJS</stitle><addtitle>Astrophys. J. Suppl</addtitle><date>2024-03-01</date><risdate>2024</risdate><volume>271</volume><issue>1</issue><spage>1</spage><pages>1-</pages><issn>0067-0049</issn><eissn>1538-4365</eissn><abstract>Thick disks are a prevalent feature observed in numerous disk galaxies, including our own Milky Way. Their significance has been reported to vary widely, ranging from a few percent to 100% of the disk mass, depending on the galaxy and the measurement method. We use the NewHorizon simulation, which has high spatial and stellar mass resolutions, to investigate the issue of the thick-disk mass fraction. We also use the NewHorizon2 simulation, which was run on the same initial conditions, but additionally traced nine chemical elements. Based on a sample of 27 massive disk galaxies with
M
*
> 10
10
M
⊙
in NewHorizon, the contribution of the thick disk was found to be 20% ± 11% in
r
-band luminosity or 35% ± 15% in mass to the overall galactic disk, which seems in agreement with observational data. The vertical profiles of 0, 22, and 5 galaxies are best fitted by 1, 2, or 3
sech
2
components, respectively. The NewHorizon2 data show that the selection of thick-disk stars based on a single [
α
/Fe] cut is contaminated by stars of different kinematic properties, while missing the bulk of kinematically thick disk stars. Vertical luminosity profile fits recover the key properties of thick disks reasonably well. The majority of stars are born near the galactic midplane with high circularity and get heated with time via fluctuations in the force field. Depending on the star formation and merger histories, galaxies may naturally develop thick disks with significantly different properties.</abstract><cop>Saskatoon</cop><pub>The American Astronomical Society</pub><doi>10.3847/1538-4365/ad0e71</doi><tpages>25</tpages><orcidid>https://orcid.org/0000-0003-0695-6735</orcidid><orcidid>https://orcid.org/0000-0002-4556-2619</orcidid><orcidid>https://orcid.org/0000-0002-3950-3997</orcidid><orcidid>https://orcid.org/0000-0002-8435-9402</orcidid><orcidid>https://orcid.org/0000-0002-8140-0422</orcidid><orcidid>https://orcid.org/0000-0002-0184-9589</orcidid><orcidid>https://orcid.org/0000-0002-0858-5264</orcidid><orcidid>https://orcid.org/0000-0001-9939-713X</orcidid><orcidid>https://orcid.org/0000-0003-0225-6387</orcidid><orcidid>https://orcid.org/0000-0001-6180-0245</orcidid><oa>free_for_read</oa></addata></record> |
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| subjects | Chemical elements Disk galaxies Galactic disk Galaxies Galaxy chemical evolution Galaxy disks Galaxy stellar disks Galaxy structure Hydrodynamical simulations Initial conditions Kinematics Luminosity Measurement methods Milky Way Sciences of the Universe Star & galaxy formation Star formation Stars Stars & galaxies Stellar mass |
| title | On the Significance of the Thick Disks of Disk Galaxies |
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