CLASS 0 PROTOSTARS IN THE PERSEUS MOLECULAR CLOUD: A CORRELATION BETWEEN THE YOUNGEST PROTOSTARS AND THE DENSE GAS DISTRIBUTION
We use PACS and SPIRE continuum data at 160 mu m, 250 mu m, 350 mu m, and 500 mu m from the Herschel Gould Belt Survey to sample seven clumps in Perseus: B1, B1-E, B5, IC 348, L1448, L1455, and NGC 1333. Additionally, we identify and characterize the embedded Class 0 protostars using detections of c...
Gespeichert in:
| Veröffentlicht in: | Astrophysical journal. Letters 2014-06, Vol.787 (2), p.1-6 |
|---|---|
| Hauptverfasser: | , , , , , , , , , |
| Format: | Artikel |
| Sprache: | eng |
| Schlagworte: | |
| Online-Zugang: | Volltext |
| Tags: |
Tag hinzufügen
Keine Tags, Fügen Sie den ersten Tag hinzu!
|
| container_end_page | 6 |
|---|---|
| container_issue | 2 |
| container_start_page | 1 |
| container_title | Astrophysical journal. Letters |
| container_volume | 787 |
| creator | Sadavoy, S I Di Francesco, J Andre, Ph Pezzuto, S Bernard, J-p Maury, A MEN'SHCHIKOV, A Motte, F NGUYEN-LU'O'NG, Q Schneider, N |
| description | We use PACS and SPIRE continuum data at 160 mu m, 250 mu m, 350 mu m, and 500 mu m from the Herschel Gould Belt Survey to sample seven clumps in Perseus: B1, B1-E, B5, IC 348, L1448, L1455, and NGC 1333. Additionally, we identify and characterize the embedded Class 0 protostars using detections of compact Herschel sources at 70 mu m as well as archival Spitzer catalogs and SCUBA 850 mu m photometric data. We identify 28 candidate Class 0 protostars, four of which are newly discovered sources not identified with Spitzer. We find that the star formation efficiency of clumps, as traced by Class 0 protostars, correlates strongly with the flatness of their respective column density distributions at high values. This correlation suggests that the fraction of high column density material in a clump reflects only its youngest protostellar population rather than its entire source population. We propose that feedback from either the formation or evolution of protostars changes the local density structure of clumps. |
| doi_str_mv | 10.1088/2041-8205/787/2/L18 |
| format | Article |
| fullrecord | <record><control><sourceid>proquest_osti_</sourceid><recordid>TN_cdi_osti_scitechconnect_22365832</recordid><sourceformat>XML</sourceformat><sourcesystem>PC</sourcesystem><sourcerecordid>1669910075</sourcerecordid><originalsourceid>FETCH-LOGICAL-c488t-b597164bf2aef935e7af1586ccd09a8218739591eeb92367aa7ef0933e69ca3</originalsourceid><addsrcrecordid>eNqNkU1v1DAQhiMEEqXwC7hY4gKHZcd2PmxubtbsRjJJFSdCnCyvcdSg7aaNUyRO_HUSUlUcOdmaed6xR08UvcXwEQNjWwIx3jACyTZj2ZZsFWbPoovHKqbPn-6QvIxehfADgECK2UX0O1dCawTouq6aSjei1qgoUXOQ6FrWWrYafamUzFslapSrqt19QgLlVV1LJZqiKtGVbL5KuUa-VW25l7r5d5ood397O1lqifZCo12hm7q4apf46-hFZ0_Bv3k8LyP9WTb5YaOqfZELtXExY9PmmPAMp_GxI9Z3nCY-sx1OWOrcd-B23pFllCcce3_khKaZtZnvgFPqU-4svYzerVOHMPUmuH7y7sYN57N3kyFzIGGUzNSHlbqxJ3M39rd2_GUG25uDUGapAfD5nZT8xDP7fmXvxuH-wYfJ3PbB-dPJnv3wEAxOU84xQJb8DxoToJzHM0pX1I1DCKPvnr6BwSymzeLRLB7NbNoQM5umfwBjuo8O</addsrcrecordid><sourcetype>Open Access Repository</sourcetype><iscdi>true</iscdi><recordtype>article</recordtype><pqid>1664203994</pqid></control><display><type>article</type><title>CLASS 0 PROTOSTARS IN THE PERSEUS MOLECULAR CLOUD: A CORRELATION BETWEEN THE YOUNGEST PROTOSTARS AND THE DENSE GAS DISTRIBUTION</title><source>IOP Publishing Free Content</source><source>Institute of Physics IOPscience extra</source><source>EZB-FREE-00999 freely available EZB journals</source><source>Alma/SFX Local Collection</source><creator>Sadavoy, S I ; Di Francesco, J ; Andre, Ph ; Pezzuto, S ; Bernard, J-p ; Maury, A ; MEN'SHCHIKOV, A ; Motte, F ; NGUYEN-LU'O'NG, Q ; Schneider, N</creator><creatorcontrib>Sadavoy, S I ; Di Francesco, J ; Andre, Ph ; Pezzuto, S ; Bernard, J-p ; Maury, A ; MEN'SHCHIKOV, A ; Motte, F ; NGUYEN-LU'O'NG, Q ; Schneider, N</creatorcontrib><description>We use PACS and SPIRE continuum data at 160 mu m, 250 mu m, 350 mu m, and 500 mu m from the Herschel Gould Belt Survey to sample seven clumps in Perseus: B1, B1-E, B5, IC 348, L1448, L1455, and NGC 1333. Additionally, we identify and characterize the embedded Class 0 protostars using detections of compact Herschel sources at 70 mu m as well as archival Spitzer catalogs and SCUBA 850 mu m photometric data. We identify 28 candidate Class 0 protostars, four of which are newly discovered sources not identified with Spitzer. We find that the star formation efficiency of clumps, as traced by Class 0 protostars, correlates strongly with the flatness of their respective column density distributions at high values. This correlation suggests that the fraction of high column density material in a clump reflects only its youngest protostellar population rather than its entire source population. We propose that feedback from either the formation or evolution of protostars changes the local density structure of clumps.</description><identifier>ISSN: 2041-8205</identifier><identifier>EISSN: 2041-8213</identifier><identifier>DOI: 10.1088/2041-8205/787/2/L18</identifier><language>eng</language><publisher>United States: Bristol : IOP Publishing</publisher><subject>Astrophysics ; ASTROPHYSICS, COSMOLOGY AND ASTRONOMY ; CLOUDS ; Clumps ; Columns (structural) ; Correlation ; COSMIC DUST ; DENSITY ; Density distribution ; DETECTION ; EFFICIENCY ; FEEDBACK ; Photometry ; Physics ; PROTOSTARS ; Sciences of the Universe ; Solar and Stellar Astrophysics ; STAR CLUSTERS ; STAR EVOLUTION ; Star formation ; STARS</subject><ispartof>Astrophysical journal. Letters, 2014-06, Vol.787 (2), p.1-6</ispartof><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-c488t-b597164bf2aef935e7af1586ccd09a8218739591eeb92367aa7ef0933e69ca3</citedby><cites>FETCH-LOGICAL-c488t-b597164bf2aef935e7af1586ccd09a8218739591eeb92367aa7ef0933e69ca3</cites><orcidid>0000-0002-3413-2293 ; 0000-0003-4574-1585 ; 0000-0002-9289-2450 ; 0000-0003-3485-6678 ; 0000-0001-7852-1971 ; 0000-0002-3597-7263 ; 0000-0002-4093-7178 ; 0000-0002-1959-7201</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>230,314,776,780,881,27903,27904</link.rule.ids><backlink>$$Uhttps://hal.science/hal-00987362$$DView record in HAL$$Hfree_for_read</backlink><backlink>$$Uhttps://www.osti.gov/biblio/22365832$$D View this record in Osti.gov$$Hfree_for_read</backlink></links><search><creatorcontrib>Sadavoy, S I</creatorcontrib><creatorcontrib>Di Francesco, J</creatorcontrib><creatorcontrib>Andre, Ph</creatorcontrib><creatorcontrib>Pezzuto, S</creatorcontrib><creatorcontrib>Bernard, J-p</creatorcontrib><creatorcontrib>Maury, A</creatorcontrib><creatorcontrib>MEN'SHCHIKOV, A</creatorcontrib><creatorcontrib>Motte, F</creatorcontrib><creatorcontrib>NGUYEN-LU'O'NG, Q</creatorcontrib><creatorcontrib>Schneider, N</creatorcontrib><title>CLASS 0 PROTOSTARS IN THE PERSEUS MOLECULAR CLOUD: A CORRELATION BETWEEN THE YOUNGEST PROTOSTARS AND THE DENSE GAS DISTRIBUTION</title><title>Astrophysical journal. Letters</title><description>We use PACS and SPIRE continuum data at 160 mu m, 250 mu m, 350 mu m, and 500 mu m from the Herschel Gould Belt Survey to sample seven clumps in Perseus: B1, B1-E, B5, IC 348, L1448, L1455, and NGC 1333. Additionally, we identify and characterize the embedded Class 0 protostars using detections of compact Herschel sources at 70 mu m as well as archival Spitzer catalogs and SCUBA 850 mu m photometric data. We identify 28 candidate Class 0 protostars, four of which are newly discovered sources not identified with Spitzer. We find that the star formation efficiency of clumps, as traced by Class 0 protostars, correlates strongly with the flatness of their respective column density distributions at high values. This correlation suggests that the fraction of high column density material in a clump reflects only its youngest protostellar population rather than its entire source population. We propose that feedback from either the formation or evolution of protostars changes the local density structure of clumps.</description><subject>Astrophysics</subject><subject>ASTROPHYSICS, COSMOLOGY AND ASTRONOMY</subject><subject>CLOUDS</subject><subject>Clumps</subject><subject>Columns (structural)</subject><subject>Correlation</subject><subject>COSMIC DUST</subject><subject>DENSITY</subject><subject>Density distribution</subject><subject>DETECTION</subject><subject>EFFICIENCY</subject><subject>FEEDBACK</subject><subject>Photometry</subject><subject>Physics</subject><subject>PROTOSTARS</subject><subject>Sciences of the Universe</subject><subject>Solar and Stellar Astrophysics</subject><subject>STAR CLUSTERS</subject><subject>STAR EVOLUTION</subject><subject>Star formation</subject><subject>STARS</subject><issn>2041-8205</issn><issn>2041-8213</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2014</creationdate><recordtype>article</recordtype><recordid>eNqNkU1v1DAQhiMEEqXwC7hY4gKHZcd2PmxubtbsRjJJFSdCnCyvcdSg7aaNUyRO_HUSUlUcOdmaed6xR08UvcXwEQNjWwIx3jACyTZj2ZZsFWbPoovHKqbPn-6QvIxehfADgECK2UX0O1dCawTouq6aSjei1qgoUXOQ6FrWWrYafamUzFslapSrqt19QgLlVV1LJZqiKtGVbL5KuUa-VW25l7r5d5ood397O1lqifZCo12hm7q4apf46-hFZ0_Bv3k8LyP9WTb5YaOqfZELtXExY9PmmPAMp_GxI9Z3nCY-sx1OWOrcd-B23pFllCcce3_khKaZtZnvgFPqU-4svYzerVOHMPUmuH7y7sYN57N3kyFzIGGUzNSHlbqxJ3M39rd2_GUG25uDUGapAfD5nZT8xDP7fmXvxuH-wYfJ3PbB-dPJnv3wEAxOU84xQJb8DxoToJzHM0pX1I1DCKPvnr6BwSymzeLRLB7NbNoQM5umfwBjuo8O</recordid><startdate>20140601</startdate><enddate>20140601</enddate><creator>Sadavoy, S I</creator><creator>Di Francesco, J</creator><creator>Andre, Ph</creator><creator>Pezzuto, S</creator><creator>Bernard, J-p</creator><creator>Maury, A</creator><creator>MEN'SHCHIKOV, A</creator><creator>Motte, F</creator><creator>NGUYEN-LU'O'NG, Q</creator><creator>Schneider, N</creator><general>Bristol : IOP Publishing</general><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>KL.</scope><scope>8FD</scope><scope>H8D</scope><scope>L7M</scope><scope>1XC</scope><scope>OTOTI</scope><orcidid>https://orcid.org/0000-0002-3413-2293</orcidid><orcidid>https://orcid.org/0000-0003-4574-1585</orcidid><orcidid>https://orcid.org/0000-0002-9289-2450</orcidid><orcidid>https://orcid.org/0000-0003-3485-6678</orcidid><orcidid>https://orcid.org/0000-0001-7852-1971</orcidid><orcidid>https://orcid.org/0000-0002-3597-7263</orcidid><orcidid>https://orcid.org/0000-0002-4093-7178</orcidid><orcidid>https://orcid.org/0000-0002-1959-7201</orcidid></search><sort><creationdate>20140601</creationdate><title>CLASS 0 PROTOSTARS IN THE PERSEUS MOLECULAR CLOUD: A CORRELATION BETWEEN THE YOUNGEST PROTOSTARS AND THE DENSE GAS DISTRIBUTION</title><author>Sadavoy, S I ; Di Francesco, J ; Andre, Ph ; Pezzuto, S ; Bernard, J-p ; Maury, A ; MEN'SHCHIKOV, A ; Motte, F ; NGUYEN-LU'O'NG, Q ; Schneider, N</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c488t-b597164bf2aef935e7af1586ccd09a8218739591eeb92367aa7ef0933e69ca3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2014</creationdate><topic>Astrophysics</topic><topic>ASTROPHYSICS, COSMOLOGY AND ASTRONOMY</topic><topic>CLOUDS</topic><topic>Clumps</topic><topic>Columns (structural)</topic><topic>Correlation</topic><topic>COSMIC DUST</topic><topic>DENSITY</topic><topic>Density distribution</topic><topic>DETECTION</topic><topic>EFFICIENCY</topic><topic>FEEDBACK</topic><topic>Photometry</topic><topic>Physics</topic><topic>PROTOSTARS</topic><topic>Sciences of the Universe</topic><topic>Solar and Stellar Astrophysics</topic><topic>STAR CLUSTERS</topic><topic>STAR EVOLUTION</topic><topic>Star formation</topic><topic>STARS</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Sadavoy, S I</creatorcontrib><creatorcontrib>Di Francesco, J</creatorcontrib><creatorcontrib>Andre, Ph</creatorcontrib><creatorcontrib>Pezzuto, S</creatorcontrib><creatorcontrib>Bernard, J-p</creatorcontrib><creatorcontrib>Maury, A</creatorcontrib><creatorcontrib>MEN'SHCHIKOV, A</creatorcontrib><creatorcontrib>Motte, F</creatorcontrib><creatorcontrib>NGUYEN-LU'O'NG, Q</creatorcontrib><creatorcontrib>Schneider, N</creatorcontrib><collection>CrossRef</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>Hyper Article en Ligne (HAL)</collection><collection>OSTI.GOV</collection><jtitle>Astrophysical journal. Letters</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Sadavoy, S I</au><au>Di Francesco, J</au><au>Andre, Ph</au><au>Pezzuto, S</au><au>Bernard, J-p</au><au>Maury, A</au><au>MEN'SHCHIKOV, A</au><au>Motte, F</au><au>NGUYEN-LU'O'NG, Q</au><au>Schneider, N</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>CLASS 0 PROTOSTARS IN THE PERSEUS MOLECULAR CLOUD: A CORRELATION BETWEEN THE YOUNGEST PROTOSTARS AND THE DENSE GAS DISTRIBUTION</atitle><jtitle>Astrophysical journal. Letters</jtitle><date>2014-06-01</date><risdate>2014</risdate><volume>787</volume><issue>2</issue><spage>1</spage><epage>6</epage><pages>1-6</pages><issn>2041-8205</issn><eissn>2041-8213</eissn><abstract>We use PACS and SPIRE continuum data at 160 mu m, 250 mu m, 350 mu m, and 500 mu m from the Herschel Gould Belt Survey to sample seven clumps in Perseus: B1, B1-E, B5, IC 348, L1448, L1455, and NGC 1333. Additionally, we identify and characterize the embedded Class 0 protostars using detections of compact Herschel sources at 70 mu m as well as archival Spitzer catalogs and SCUBA 850 mu m photometric data. We identify 28 candidate Class 0 protostars, four of which are newly discovered sources not identified with Spitzer. We find that the star formation efficiency of clumps, as traced by Class 0 protostars, correlates strongly with the flatness of their respective column density distributions at high values. This correlation suggests that the fraction of high column density material in a clump reflects only its youngest protostellar population rather than its entire source population. We propose that feedback from either the formation or evolution of protostars changes the local density structure of clumps.</abstract><cop>United States</cop><pub>Bristol : IOP Publishing</pub><doi>10.1088/2041-8205/787/2/L18</doi><tpages>6</tpages><orcidid>https://orcid.org/0000-0002-3413-2293</orcidid><orcidid>https://orcid.org/0000-0003-4574-1585</orcidid><orcidid>https://orcid.org/0000-0002-9289-2450</orcidid><orcidid>https://orcid.org/0000-0003-3485-6678</orcidid><orcidid>https://orcid.org/0000-0001-7852-1971</orcidid><orcidid>https://orcid.org/0000-0002-3597-7263</orcidid><orcidid>https://orcid.org/0000-0002-4093-7178</orcidid><orcidid>https://orcid.org/0000-0002-1959-7201</orcidid><oa>free_for_read</oa></addata></record> |
| fulltext | fulltext |
| identifier | ISSN: 2041-8205 |
| ispartof | Astrophysical journal. Letters, 2014-06, Vol.787 (2), p.1-6 |
| issn | 2041-8205 2041-8213 |
| language | eng |
| recordid | cdi_osti_scitechconnect_22365832 |
| source | IOP Publishing Free Content; Institute of Physics IOPscience extra; EZB-FREE-00999 freely available EZB journals; Alma/SFX Local Collection |
| subjects | Astrophysics ASTROPHYSICS, COSMOLOGY AND ASTRONOMY CLOUDS Clumps Columns (structural) Correlation COSMIC DUST DENSITY Density distribution DETECTION EFFICIENCY FEEDBACK Photometry Physics PROTOSTARS Sciences of the Universe Solar and Stellar Astrophysics STAR CLUSTERS STAR EVOLUTION Star formation STARS |
| title | CLASS 0 PROTOSTARS IN THE PERSEUS MOLECULAR CLOUD: A CORRELATION BETWEEN THE YOUNGEST PROTOSTARS AND THE DENSE GAS DISTRIBUTION |
| url | https://sfx.bib-bvb.de/sfx_tum?ctx_ver=Z39.88-2004&ctx_enc=info:ofi/enc:UTF-8&ctx_tim=2025-01-22T08%3A51%3A48IST&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=CLASS%200%20PROTOSTARS%20IN%20THE%20PERSEUS%20MOLECULAR%20CLOUD:%20A%20CORRELATION%20BETWEEN%20THE%20YOUNGEST%20PROTOSTARS%20AND%20THE%20DENSE%20GAS%20DISTRIBUTION&rft.jtitle=Astrophysical%20journal.%20Letters&rft.au=Sadavoy,%20S%20I&rft.date=2014-06-01&rft.volume=787&rft.issue=2&rft.spage=1&rft.epage=6&rft.pages=1-6&rft.issn=2041-8205&rft.eissn=2041-8213&rft_id=info:doi/10.1088/2041-8205/787/2/L18&rft_dat=%3Cproquest_osti_%3E1669910075%3C/proquest_osti_%3E%3Curl%3E%3C/url%3E&disable_directlink=true&sfx.directlink=off&sfx.report_link=0&rft_id=info:oai/&rft_pqid=1664203994&rft_id=info:pmid/&rfr_iscdi=true |