On the duration of the embedded phase of star formation
ABSTRACT Feedback from massive stars plays a key role in molecular cloud evolution. After the onset of star formation, the young stellar population is exposed by photoionization, winds, supernovae, and radiation pressure from massive stars. Recent observations of nearby galaxies have provided the ev...
Gespeichert in:
Veröffentlicht in: | Monthly notices of the Royal Astronomical Society 2021-06, Vol.504 (1), p.487-509 |
---|---|
Hauptverfasser: | , , , , , , , , , , , , , , , , , , , , , , , , , |
Format: | Artikel |
Sprache: | eng |
Schlagworte: | |
Online-Zugang: | Volltext bestellen |
Tags: |
Tag hinzufügen
Keine Tags, Fügen Sie den ersten Tag hinzu!
|
container_end_page | 509 |
---|---|
container_issue | 1 |
container_start_page | 487 |
container_title | Monthly notices of the Royal Astronomical Society |
container_volume | 504 |
creator | Kim, Jaeyeon Chevance, Mélanie Kruijssen, J M Diederik Schruba, Andreas Sandstrom, Karin Barnes, Ashley T Bigiel, Frank Blanc, Guillermo A Cao, Yixian Dale, Daniel A Faesi, Christopher M Glover, Simon C O Grasha, Kathryn Groves, Brent Herrera, Cinthya Klessen, Ralf S Kreckel, Kathryn Lee, Janice C Leroy, Adam K Pety, Jérôme Querejeta, Miguel Schinnerer, Eva Sun, Jiayi Usero, Antonio Ward, Jacob L Williams, Thomas G |
description | ABSTRACT
Feedback from massive stars plays a key role in molecular cloud evolution. After the onset of star formation, the young stellar population is exposed by photoionization, winds, supernovae, and radiation pressure from massive stars. Recent observations of nearby galaxies have provided the evolutionary timeline between molecular clouds and exposed young stars, but the duration of the embedded phase of massive star formation is still ill-constrained. We measure how long massive stellar populations remain embedded within their natal cloud, by applying a statistical method to six nearby galaxies at $20{-}100~\mbox{${\rm ~pc}$}$ resolution, using CO, Spitzer 24$\rm \, \mu m$, and H α emission as tracers of molecular clouds, embedded star formation, and exposed star formation, respectively. We find that the embedded phase (with CO and 24$\rm \, \mu m$ emission) lasts for 2−7 Myr and constitutes $17{-}47{{\ \rm per\ cent}}$ of the cloud lifetime. During approximately the first half of this phase, the region is invisible in H α, making it heavily obscured. For the second half of this phase, the region also emits in H α and is partially exposed. Once the cloud has been dispersed by feedback, 24$\rm \, \mu m$ emission no longer traces ongoing star formation, but remains detectable for another 2−9 Myr through the emission from ambient CO-dark gas, tracing star formation that recently ended. The short duration of massive star formation suggests that pre-supernova feedback (photoionization and winds) is important in disrupting molecular clouds. The measured time-scales do not show significant correlations with environmental properties (e.g. metallicity). Future JWST observations will enable these measurements routinely across the nearby galaxy population. |
doi_str_mv | 10.1093/mnras/stab878 |
format | Article |
fullrecord | <record><control><sourceid>oup_TOX</sourceid><recordid>TN_cdi_hal_primary_oai_HAL_hal_03482867v1</recordid><sourceformat>XML</sourceformat><sourcesystem>PC</sourcesystem><oup_id>10.1093/mnras/stab878</oup_id><sourcerecordid>10.1093/mnras/stab878</sourcerecordid><originalsourceid>FETCH-LOGICAL-c409t-764d0fe4661cc8a92de8e614c091e897b1869747204b3d78dd46dc914d8d8f883</originalsourceid><addsrcrecordid>eNqFkDtPwzAUhS0EEqEwsmeEIfQ6du3rsaqgRYrUBWbLiR0lqHnITpH49-RRsTJd3aPvnOEj5JHCCwXF1k3rTViHweQo8YpElIlNkiohrkkEwDYJSkpvyV0IXwDAWSoiIo9tPFQutmdvhrpr466cf9fkzlpn474ywU3puOvjsvPNzN2Tm9Kcgnu43BX5fHv92B2S7Lh_322zpOCghkQKbqF0XAhaFGhUah06QXkBijpUMqcolOQyBZ4zK9FaLmyhKLdosURkK_K87FbmpHtfN8b_6M7U-rDN9JQB45iikN90ZJOFLXwXgnflX4GCngzp2ZC-GBr5p4Xvzv0_6C_k02fS</addsrcrecordid><sourcetype>Open Access Repository</sourcetype><iscdi>true</iscdi><recordtype>article</recordtype></control><display><type>article</type><title>On the duration of the embedded phase of star formation</title><source>Oxford Journals Open Access Collection</source><creator>Kim, Jaeyeon ; Chevance, Mélanie ; Kruijssen, J M Diederik ; Schruba, Andreas ; Sandstrom, Karin ; Barnes, Ashley T ; Bigiel, Frank ; Blanc, Guillermo A ; Cao, Yixian ; Dale, Daniel A ; Faesi, Christopher M ; Glover, Simon C O ; Grasha, Kathryn ; Groves, Brent ; Herrera, Cinthya ; Klessen, Ralf S ; Kreckel, Kathryn ; Lee, Janice C ; Leroy, Adam K ; Pety, Jérôme ; Querejeta, Miguel ; Schinnerer, Eva ; Sun, Jiayi ; Usero, Antonio ; Ward, Jacob L ; Williams, Thomas G</creator><creatorcontrib>Kim, Jaeyeon ; Chevance, Mélanie ; Kruijssen, J M Diederik ; Schruba, Andreas ; Sandstrom, Karin ; Barnes, Ashley T ; Bigiel, Frank ; Blanc, Guillermo A ; Cao, Yixian ; Dale, Daniel A ; Faesi, Christopher M ; Glover, Simon C O ; Grasha, Kathryn ; Groves, Brent ; Herrera, Cinthya ; Klessen, Ralf S ; Kreckel, Kathryn ; Lee, Janice C ; Leroy, Adam K ; Pety, Jérôme ; Querejeta, Miguel ; Schinnerer, Eva ; Sun, Jiayi ; Usero, Antonio ; Ward, Jacob L ; Williams, Thomas G</creatorcontrib><description>ABSTRACT
Feedback from massive stars plays a key role in molecular cloud evolution. After the onset of star formation, the young stellar population is exposed by photoionization, winds, supernovae, and radiation pressure from massive stars. Recent observations of nearby galaxies have provided the evolutionary timeline between molecular clouds and exposed young stars, but the duration of the embedded phase of massive star formation is still ill-constrained. We measure how long massive stellar populations remain embedded within their natal cloud, by applying a statistical method to six nearby galaxies at $20{-}100~\mbox{${\rm ~pc}$}$ resolution, using CO, Spitzer 24$\rm \, \mu m$, and H α emission as tracers of molecular clouds, embedded star formation, and exposed star formation, respectively. We find that the embedded phase (with CO and 24$\rm \, \mu m$ emission) lasts for 2−7 Myr and constitutes $17{-}47{{\ \rm per\ cent}}$ of the cloud lifetime. During approximately the first half of this phase, the region is invisible in H α, making it heavily obscured. For the second half of this phase, the region also emits in H α and is partially exposed. Once the cloud has been dispersed by feedback, 24$\rm \, \mu m$ emission no longer traces ongoing star formation, but remains detectable for another 2−9 Myr through the emission from ambient CO-dark gas, tracing star formation that recently ended. The short duration of massive star formation suggests that pre-supernova feedback (photoionization and winds) is important in disrupting molecular clouds. The measured time-scales do not show significant correlations with environmental properties (e.g. metallicity). Future JWST observations will enable these measurements routinely across the nearby galaxy population.</description><identifier>ISSN: 0035-8711</identifier><identifier>EISSN: 1365-2966</identifier><identifier>DOI: 10.1093/mnras/stab878</identifier><language>eng</language><publisher>Oxford University Press</publisher><subject>Astrophysics ; Physics</subject><ispartof>Monthly notices of the Royal Astronomical Society, 2021-06, Vol.504 (1), p.487-509</ispartof><rights>2021 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society 2021</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-c409t-764d0fe4661cc8a92de8e614c091e897b1869747204b3d78dd46dc914d8d8f883</citedby><cites>FETCH-LOGICAL-c409t-764d0fe4661cc8a92de8e614c091e897b1869747204b3d78dd46dc914d8d8f883</cites><orcidid>0000-0001-6708-1317 ; 0000-0003-0378-4667 ; 0000-0002-0432-6847 ; 0000-0003-0410-4504 ; 0000-0002-8804-0212 ; 0000-0002-3247-5321 ; 0000-0002-5635-5180 ; 0000-0002-0560-3172 ; 0000-0001-6551-3091 ; 0000-0002-0012-2142 ; 0000-0002-5841-0649 ; 0000-0002-0472-1011 ; 0000-0002-5782-9093 ; 0000-0002-3933-7677 ; 0000-0003-1242-505X ; 0000-0002-9768-0246 ; 0000-0001-5301-1326 ; 0000-0003-4218-3944 ; 0000-0003-3061-6546 ; 0000-0002-2545-1700 ; 0000-0002-4378-8534 ; 0000-0003-0166-9745 ; 0000-0001-5310-467X ; 0000-0002-2278-9407 ; 0000-0001-6405-0785</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>230,314,776,780,881,1598,27901,27902</link.rule.ids><linktorsrc>$$Uhttps://dx.doi.org/10.1093/mnras/stab878$$EView_record_in_Oxford_University_Press$$FView_record_in_$$GOxford_University_Press</linktorsrc><backlink>$$Uhttps://hal.science/hal-03482867$$DView record in HAL$$Hfree_for_read</backlink></links><search><creatorcontrib>Kim, Jaeyeon</creatorcontrib><creatorcontrib>Chevance, Mélanie</creatorcontrib><creatorcontrib>Kruijssen, J M Diederik</creatorcontrib><creatorcontrib>Schruba, Andreas</creatorcontrib><creatorcontrib>Sandstrom, Karin</creatorcontrib><creatorcontrib>Barnes, Ashley T</creatorcontrib><creatorcontrib>Bigiel, Frank</creatorcontrib><creatorcontrib>Blanc, Guillermo A</creatorcontrib><creatorcontrib>Cao, Yixian</creatorcontrib><creatorcontrib>Dale, Daniel A</creatorcontrib><creatorcontrib>Faesi, Christopher M</creatorcontrib><creatorcontrib>Glover, Simon C O</creatorcontrib><creatorcontrib>Grasha, Kathryn</creatorcontrib><creatorcontrib>Groves, Brent</creatorcontrib><creatorcontrib>Herrera, Cinthya</creatorcontrib><creatorcontrib>Klessen, Ralf S</creatorcontrib><creatorcontrib>Kreckel, Kathryn</creatorcontrib><creatorcontrib>Lee, Janice C</creatorcontrib><creatorcontrib>Leroy, Adam K</creatorcontrib><creatorcontrib>Pety, Jérôme</creatorcontrib><creatorcontrib>Querejeta, Miguel</creatorcontrib><creatorcontrib>Schinnerer, Eva</creatorcontrib><creatorcontrib>Sun, Jiayi</creatorcontrib><creatorcontrib>Usero, Antonio</creatorcontrib><creatorcontrib>Ward, Jacob L</creatorcontrib><creatorcontrib>Williams, Thomas G</creatorcontrib><title>On the duration of the embedded phase of star formation</title><title>Monthly notices of the Royal Astronomical Society</title><description>ABSTRACT
Feedback from massive stars plays a key role in molecular cloud evolution. After the onset of star formation, the young stellar population is exposed by photoionization, winds, supernovae, and radiation pressure from massive stars. Recent observations of nearby galaxies have provided the evolutionary timeline between molecular clouds and exposed young stars, but the duration of the embedded phase of massive star formation is still ill-constrained. We measure how long massive stellar populations remain embedded within their natal cloud, by applying a statistical method to six nearby galaxies at $20{-}100~\mbox{${\rm ~pc}$}$ resolution, using CO, Spitzer 24$\rm \, \mu m$, and H α emission as tracers of molecular clouds, embedded star formation, and exposed star formation, respectively. We find that the embedded phase (with CO and 24$\rm \, \mu m$ emission) lasts for 2−7 Myr and constitutes $17{-}47{{\ \rm per\ cent}}$ of the cloud lifetime. During approximately the first half of this phase, the region is invisible in H α, making it heavily obscured. For the second half of this phase, the region also emits in H α and is partially exposed. Once the cloud has been dispersed by feedback, 24$\rm \, \mu m$ emission no longer traces ongoing star formation, but remains detectable for another 2−9 Myr through the emission from ambient CO-dark gas, tracing star formation that recently ended. The short duration of massive star formation suggests that pre-supernova feedback (photoionization and winds) is important in disrupting molecular clouds. The measured time-scales do not show significant correlations with environmental properties (e.g. metallicity). Future JWST observations will enable these measurements routinely across the nearby galaxy population.</description><subject>Astrophysics</subject><subject>Physics</subject><issn>0035-8711</issn><issn>1365-2966</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2021</creationdate><recordtype>article</recordtype><recordid>eNqFkDtPwzAUhS0EEqEwsmeEIfQ6du3rsaqgRYrUBWbLiR0lqHnITpH49-RRsTJd3aPvnOEj5JHCCwXF1k3rTViHweQo8YpElIlNkiohrkkEwDYJSkpvyV0IXwDAWSoiIo9tPFQutmdvhrpr466cf9fkzlpn474ywU3puOvjsvPNzN2Tm9Kcgnu43BX5fHv92B2S7Lh_322zpOCghkQKbqF0XAhaFGhUah06QXkBijpUMqcolOQyBZ4zK9FaLmyhKLdosURkK_K87FbmpHtfN8b_6M7U-rDN9JQB45iikN90ZJOFLXwXgnflX4GCngzp2ZC-GBr5p4Xvzv0_6C_k02fS</recordid><startdate>20210601</startdate><enddate>20210601</enddate><creator>Kim, Jaeyeon</creator><creator>Chevance, Mélanie</creator><creator>Kruijssen, J M Diederik</creator><creator>Schruba, Andreas</creator><creator>Sandstrom, Karin</creator><creator>Barnes, Ashley T</creator><creator>Bigiel, Frank</creator><creator>Blanc, Guillermo A</creator><creator>Cao, Yixian</creator><creator>Dale, Daniel A</creator><creator>Faesi, Christopher M</creator><creator>Glover, Simon C O</creator><creator>Grasha, Kathryn</creator><creator>Groves, Brent</creator><creator>Herrera, Cinthya</creator><creator>Klessen, Ralf S</creator><creator>Kreckel, Kathryn</creator><creator>Lee, Janice C</creator><creator>Leroy, Adam K</creator><creator>Pety, Jérôme</creator><creator>Querejeta, Miguel</creator><creator>Schinnerer, Eva</creator><creator>Sun, Jiayi</creator><creator>Usero, Antonio</creator><creator>Ward, Jacob L</creator><creator>Williams, Thomas G</creator><general>Oxford University Press</general><general>Oxford University Press (OUP): Policy P - Oxford Open Option A</general><scope>AAYXX</scope><scope>CITATION</scope><scope>1XC</scope><scope>VOOES</scope><orcidid>https://orcid.org/0000-0001-6708-1317</orcidid><orcidid>https://orcid.org/0000-0003-0378-4667</orcidid><orcidid>https://orcid.org/0000-0002-0432-6847</orcidid><orcidid>https://orcid.org/0000-0003-0410-4504</orcidid><orcidid>https://orcid.org/0000-0002-8804-0212</orcidid><orcidid>https://orcid.org/0000-0002-3247-5321</orcidid><orcidid>https://orcid.org/0000-0002-5635-5180</orcidid><orcidid>https://orcid.org/0000-0002-0560-3172</orcidid><orcidid>https://orcid.org/0000-0001-6551-3091</orcidid><orcidid>https://orcid.org/0000-0002-0012-2142</orcidid><orcidid>https://orcid.org/0000-0002-5841-0649</orcidid><orcidid>https://orcid.org/0000-0002-0472-1011</orcidid><orcidid>https://orcid.org/0000-0002-5782-9093</orcidid><orcidid>https://orcid.org/0000-0002-3933-7677</orcidid><orcidid>https://orcid.org/0000-0003-1242-505X</orcidid><orcidid>https://orcid.org/0000-0002-9768-0246</orcidid><orcidid>https://orcid.org/0000-0001-5301-1326</orcidid><orcidid>https://orcid.org/0000-0003-4218-3944</orcidid><orcidid>https://orcid.org/0000-0003-3061-6546</orcidid><orcidid>https://orcid.org/0000-0002-2545-1700</orcidid><orcidid>https://orcid.org/0000-0002-4378-8534</orcidid><orcidid>https://orcid.org/0000-0003-0166-9745</orcidid><orcidid>https://orcid.org/0000-0001-5310-467X</orcidid><orcidid>https://orcid.org/0000-0002-2278-9407</orcidid><orcidid>https://orcid.org/0000-0001-6405-0785</orcidid></search><sort><creationdate>20210601</creationdate><title>On the duration of the embedded phase of star formation</title><author>Kim, Jaeyeon ; Chevance, Mélanie ; Kruijssen, J M Diederik ; Schruba, Andreas ; Sandstrom, Karin ; Barnes, Ashley T ; Bigiel, Frank ; Blanc, Guillermo A ; Cao, Yixian ; Dale, Daniel A ; Faesi, Christopher M ; Glover, Simon C O ; Grasha, Kathryn ; Groves, Brent ; Herrera, Cinthya ; Klessen, Ralf S ; Kreckel, Kathryn ; Lee, Janice C ; Leroy, Adam K ; Pety, Jérôme ; Querejeta, Miguel ; Schinnerer, Eva ; Sun, Jiayi ; Usero, Antonio ; Ward, Jacob L ; Williams, Thomas G</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c409t-764d0fe4661cc8a92de8e614c091e897b1869747204b3d78dd46dc914d8d8f883</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2021</creationdate><topic>Astrophysics</topic><topic>Physics</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Kim, Jaeyeon</creatorcontrib><creatorcontrib>Chevance, Mélanie</creatorcontrib><creatorcontrib>Kruijssen, J M Diederik</creatorcontrib><creatorcontrib>Schruba, Andreas</creatorcontrib><creatorcontrib>Sandstrom, Karin</creatorcontrib><creatorcontrib>Barnes, Ashley T</creatorcontrib><creatorcontrib>Bigiel, Frank</creatorcontrib><creatorcontrib>Blanc, Guillermo A</creatorcontrib><creatorcontrib>Cao, Yixian</creatorcontrib><creatorcontrib>Dale, Daniel A</creatorcontrib><creatorcontrib>Faesi, Christopher M</creatorcontrib><creatorcontrib>Glover, Simon C O</creatorcontrib><creatorcontrib>Grasha, Kathryn</creatorcontrib><creatorcontrib>Groves, Brent</creatorcontrib><creatorcontrib>Herrera, Cinthya</creatorcontrib><creatorcontrib>Klessen, Ralf S</creatorcontrib><creatorcontrib>Kreckel, Kathryn</creatorcontrib><creatorcontrib>Lee, Janice C</creatorcontrib><creatorcontrib>Leroy, Adam K</creatorcontrib><creatorcontrib>Pety, Jérôme</creatorcontrib><creatorcontrib>Querejeta, Miguel</creatorcontrib><creatorcontrib>Schinnerer, Eva</creatorcontrib><creatorcontrib>Sun, Jiayi</creatorcontrib><creatorcontrib>Usero, Antonio</creatorcontrib><creatorcontrib>Ward, Jacob L</creatorcontrib><creatorcontrib>Williams, Thomas G</creatorcontrib><collection>CrossRef</collection><collection>Hyper Article en Ligne (HAL)</collection><collection>Hyper Article en Ligne (HAL) (Open Access)</collection><jtitle>Monthly notices of the Royal Astronomical Society</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext_linktorsrc</fulltext></delivery><addata><au>Kim, Jaeyeon</au><au>Chevance, Mélanie</au><au>Kruijssen, J M Diederik</au><au>Schruba, Andreas</au><au>Sandstrom, Karin</au><au>Barnes, Ashley T</au><au>Bigiel, Frank</au><au>Blanc, Guillermo A</au><au>Cao, Yixian</au><au>Dale, Daniel A</au><au>Faesi, Christopher M</au><au>Glover, Simon C O</au><au>Grasha, Kathryn</au><au>Groves, Brent</au><au>Herrera, Cinthya</au><au>Klessen, Ralf S</au><au>Kreckel, Kathryn</au><au>Lee, Janice C</au><au>Leroy, Adam K</au><au>Pety, Jérôme</au><au>Querejeta, Miguel</au><au>Schinnerer, Eva</au><au>Sun, Jiayi</au><au>Usero, Antonio</au><au>Ward, Jacob L</au><au>Williams, Thomas G</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>On the duration of the embedded phase of star formation</atitle><jtitle>Monthly notices of the Royal Astronomical Society</jtitle><date>2021-06-01</date><risdate>2021</risdate><volume>504</volume><issue>1</issue><spage>487</spage><epage>509</epage><pages>487-509</pages><issn>0035-8711</issn><eissn>1365-2966</eissn><abstract>ABSTRACT
Feedback from massive stars plays a key role in molecular cloud evolution. After the onset of star formation, the young stellar population is exposed by photoionization, winds, supernovae, and radiation pressure from massive stars. Recent observations of nearby galaxies have provided the evolutionary timeline between molecular clouds and exposed young stars, but the duration of the embedded phase of massive star formation is still ill-constrained. We measure how long massive stellar populations remain embedded within their natal cloud, by applying a statistical method to six nearby galaxies at $20{-}100~\mbox{${\rm ~pc}$}$ resolution, using CO, Spitzer 24$\rm \, \mu m$, and H α emission as tracers of molecular clouds, embedded star formation, and exposed star formation, respectively. We find that the embedded phase (with CO and 24$\rm \, \mu m$ emission) lasts for 2−7 Myr and constitutes $17{-}47{{\ \rm per\ cent}}$ of the cloud lifetime. During approximately the first half of this phase, the region is invisible in H α, making it heavily obscured. For the second half of this phase, the region also emits in H α and is partially exposed. Once the cloud has been dispersed by feedback, 24$\rm \, \mu m$ emission no longer traces ongoing star formation, but remains detectable for another 2−9 Myr through the emission from ambient CO-dark gas, tracing star formation that recently ended. The short duration of massive star formation suggests that pre-supernova feedback (photoionization and winds) is important in disrupting molecular clouds. The measured time-scales do not show significant correlations with environmental properties (e.g. metallicity). Future JWST observations will enable these measurements routinely across the nearby galaxy population.</abstract><pub>Oxford University Press</pub><doi>10.1093/mnras/stab878</doi><tpages>23</tpages><orcidid>https://orcid.org/0000-0001-6708-1317</orcidid><orcidid>https://orcid.org/0000-0003-0378-4667</orcidid><orcidid>https://orcid.org/0000-0002-0432-6847</orcidid><orcidid>https://orcid.org/0000-0003-0410-4504</orcidid><orcidid>https://orcid.org/0000-0002-8804-0212</orcidid><orcidid>https://orcid.org/0000-0002-3247-5321</orcidid><orcidid>https://orcid.org/0000-0002-5635-5180</orcidid><orcidid>https://orcid.org/0000-0002-0560-3172</orcidid><orcidid>https://orcid.org/0000-0001-6551-3091</orcidid><orcidid>https://orcid.org/0000-0002-0012-2142</orcidid><orcidid>https://orcid.org/0000-0002-5841-0649</orcidid><orcidid>https://orcid.org/0000-0002-0472-1011</orcidid><orcidid>https://orcid.org/0000-0002-5782-9093</orcidid><orcidid>https://orcid.org/0000-0002-3933-7677</orcidid><orcidid>https://orcid.org/0000-0003-1242-505X</orcidid><orcidid>https://orcid.org/0000-0002-9768-0246</orcidid><orcidid>https://orcid.org/0000-0001-5301-1326</orcidid><orcidid>https://orcid.org/0000-0003-4218-3944</orcidid><orcidid>https://orcid.org/0000-0003-3061-6546</orcidid><orcidid>https://orcid.org/0000-0002-2545-1700</orcidid><orcidid>https://orcid.org/0000-0002-4378-8534</orcidid><orcidid>https://orcid.org/0000-0003-0166-9745</orcidid><orcidid>https://orcid.org/0000-0001-5310-467X</orcidid><orcidid>https://orcid.org/0000-0002-2278-9407</orcidid><orcidid>https://orcid.org/0000-0001-6405-0785</orcidid><oa>free_for_read</oa></addata></record> |
fulltext | fulltext_linktorsrc |
identifier | ISSN: 0035-8711 |
ispartof | Monthly notices of the Royal Astronomical Society, 2021-06, Vol.504 (1), p.487-509 |
issn | 0035-8711 1365-2966 |
language | eng |
recordid | cdi_hal_primary_oai_HAL_hal_03482867v1 |
source | Oxford Journals Open Access Collection |
subjects | Astrophysics Physics |
title | On the duration of the embedded phase of star formation |
url | https://sfx.bib-bvb.de/sfx_tum?ctx_ver=Z39.88-2004&ctx_enc=info:ofi/enc:UTF-8&ctx_tim=2025-02-07T12%3A28%3A44IST&url_ver=Z39.88-2004&url_ctx_fmt=infofi/fmt:kev:mtx:ctx&rfr_id=info:sid/primo.exlibrisgroup.com:primo3-Article-oup_TOX&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.genre=article&rft.atitle=On%20the%20duration%20of%20the%20embedded%20phase%20of%20star%20formation&rft.jtitle=Monthly%20notices%20of%20the%20Royal%20Astronomical%20Society&rft.au=Kim,%20Jaeyeon&rft.date=2021-06-01&rft.volume=504&rft.issue=1&rft.spage=487&rft.epage=509&rft.pages=487-509&rft.issn=0035-8711&rft.eissn=1365-2966&rft_id=info:doi/10.1093/mnras/stab878&rft_dat=%3Coup_TOX%3E10.1093/mnras/stab878%3C/oup_TOX%3E%3Curl%3E%3C/url%3E&disable_directlink=true&sfx.directlink=off&sfx.report_link=0&rft_id=info:oai/&rft_id=info:pmid/&rft_oup_id=10.1093/mnras/stab878&rfr_iscdi=true |