Loading…

The Herschel view of the massive star-forming region NGC 6334

Aims: Fundamental to any theory of high-mass star formation are gravity and turbulence. Their relative importance, which probably changes during cloud evolution, is not known. By investigating the spatial and density structure of the high-mass star-forming complex NGC 6334 we aim to disentangle the...

Full description

Saved in:
Bibliographic Details
Published in:Astronomy and astrophysics (Berlin) 2013-06, Vol.554
Main Authors: Russeil, D., Schneider, N., Anderson, L. D., Zavagno, Annie, Molinari, S., Persi, P., Bontemps, Sylvain, Motte, F., Ossenkopf, V., André, Ph, Arzoumanian, D., Bernard, J.-Ph, Deharveng, L., Didelon, P., Di Francesco, J., Elia, D., Hennemann, M., Hill, T., Könyves, V., Li, J. Z., Martin, P. G., Nguyen Luong, Q., Peretto, N., Pezzuto, S., Polychroni, D., Roussel, Hervé, Rygl, K. L. J., Spinoglio, L., Testi, L., Tigé, J., Vavrek, R., Ward-Thompson, D., White, G.
Format: Article
Language:English
Subjects:
Online Access:Get full text
Tags: Add Tag
No Tags, Be the first to tag this record!
cited_by
cites
container_end_page
container_issue
container_start_page
container_title Astronomy and astrophysics (Berlin)
container_volume 554
creator Russeil, D.
Schneider, N.
Anderson, L. D.
Zavagno, Annie
Molinari, S.
Persi, P.
Bontemps, Sylvain
Motte, F.
Ossenkopf, V.
André, Ph
Arzoumanian, D.
Bernard, J.-Ph
Deharveng, L.
Didelon, P.
Di Francesco, J.
Elia, D.
Hennemann, M.
Hill, T.
Könyves, V.
Li, J. Z.
Martin, P. G.
Nguyen Luong, Q.
Peretto, N.
Pezzuto, S.
Polychroni, D.
Roussel, Hervé
Rygl, K. L. J.
Spinoglio, L.
Testi, L.
Tigé, J.
Vavrek, R.
Ward-Thompson, D.
White, G.
description Aims: Fundamental to any theory of high-mass star formation are gravity and turbulence. Their relative importance, which probably changes during cloud evolution, is not known. By investigating the spatial and density structure of the high-mass star-forming complex NGC 6334 we aim to disentangle the contributions of turbulence and gravity. Methods: We used Herschel PACS and SPIRE imaging observations from the HOBYS key programme at wavelengths of 160, 250, 350, and 500 μm to construct dust temperature and column density maps. Using probability distribution functions (PDFs) of the column density determined for the whole complex and for four distinct sub-regions (distinguished on the basis of differences in the column density, temperature, and radiation field), we characterize the density structure of the complex. We investigate the spatial structure using the Δ-variance, which probes the relative amount of structure on different size scales and traces possible energy injection mechanisms into the molecular cloud. Results: The Δ-variance analysis suggests that the significant scales of a few parsec that were found are caused by energy injection due to expanding H ii regions, which are numerous, and by the lengths of filaments seen everywhere in the complex. The column density PDFs have a lognormal shape at low densities and a clearly defined power law at high densities for all sub-regions whose slope is linked to the exponent α of an equivalent spherical density distribution. In particular with α = 2.37, the central sub-region is largly dominated by gravity, caused by individual collapsing dense cores and global collapse of a larger region. The collapse is faster than free-fall (which would lead only to α = 2) and thus requires a more dynamic scenario (external compression, flows). The column density PDFs suggest that the different sub-regions are at different evolutionary stages, especially the central sub-region, which seems to be in a more evolved stage. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.Appendix A is available in electronic form at www.aanda.org
doi_str_mv 10.1051/0004-6361/201219971
format article
fullrecord <record><control><sourceid>hal</sourceid><recordid>TN_cdi_hal_primary_oai_HAL_hal_00838710v1</recordid><sourceformat>XML</sourceformat><sourcesystem>PC</sourcesystem><sourcerecordid>oai_HAL_hal_00838710v1</sourcerecordid><originalsourceid>FETCH-hal_primary_oai_HAL_hal_00838710v13</originalsourceid><addsrcrecordid>eNqVirsKwjAUQIMoWB9f4JLVIfbepk3bwUGK2kGcupcgaRvpQ5JS8e-tIO5Oh3M4hGwQdggBugDgM8EFuh6gh3Ec4oQ46HOPQRiIKXF-x5wsrL2P6mHEHbLPKkVTZeytUjUdtHrSrqD9GBtprR4Utb00rOhMo9uSGlXqrqXXc0IF5_6KzApZW7X-ckm2p2OWpKySdf4wupHmlXdS5-nhkn8aQMSjEGFA_s_7Bv3SQK0</addsrcrecordid><sourcetype>Open Access Repository</sourcetype><iscdi>true</iscdi><recordtype>article</recordtype></control><display><type>article</type><title>The Herschel view of the massive star-forming region NGC 6334</title><source>EZB Electronic Journals Library</source><creator>Russeil, D. ; Schneider, N. ; Anderson, L. D. ; Zavagno, Annie ; Molinari, S. ; Persi, P. ; Bontemps, Sylvain ; Motte, F. ; Ossenkopf, V. ; André, Ph ; Arzoumanian, D. ; Bernard, J.-Ph ; Deharveng, L. ; Didelon, P. ; Di Francesco, J. ; Elia, D. ; Hennemann, M. ; Hill, T. ; Könyves, V. ; Li, J. Z. ; Martin, P. G. ; Nguyen Luong, Q. ; Peretto, N. ; Pezzuto, S. ; Polychroni, D. ; Roussel, Hervé ; Rygl, K. L. J. ; Spinoglio, L. ; Testi, L. ; Tigé, J. ; Vavrek, R. ; Ward-Thompson, D. ; White, G.</creator><creatorcontrib>Russeil, D. ; Schneider, N. ; Anderson, L. D. ; Zavagno, Annie ; Molinari, S. ; Persi, P. ; Bontemps, Sylvain ; Motte, F. ; Ossenkopf, V. ; André, Ph ; Arzoumanian, D. ; Bernard, J.-Ph ; Deharveng, L. ; Didelon, P. ; Di Francesco, J. ; Elia, D. ; Hennemann, M. ; Hill, T. ; Könyves, V. ; Li, J. Z. ; Martin, P. G. ; Nguyen Luong, Q. ; Peretto, N. ; Pezzuto, S. ; Polychroni, D. ; Roussel, Hervé ; Rygl, K. L. J. ; Spinoglio, L. ; Testi, L. ; Tigé, J. ; Vavrek, R. ; Ward-Thompson, D. ; White, G.</creatorcontrib><description>Aims: Fundamental to any theory of high-mass star formation are gravity and turbulence. Their relative importance, which probably changes during cloud evolution, is not known. By investigating the spatial and density structure of the high-mass star-forming complex NGC 6334 we aim to disentangle the contributions of turbulence and gravity. Methods: We used Herschel PACS and SPIRE imaging observations from the HOBYS key programme at wavelengths of 160, 250, 350, and 500 μm to construct dust temperature and column density maps. Using probability distribution functions (PDFs) of the column density determined for the whole complex and for four distinct sub-regions (distinguished on the basis of differences in the column density, temperature, and radiation field), we characterize the density structure of the complex. We investigate the spatial structure using the Δ-variance, which probes the relative amount of structure on different size scales and traces possible energy injection mechanisms into the molecular cloud. Results: The Δ-variance analysis suggests that the significant scales of a few parsec that were found are caused by energy injection due to expanding H ii regions, which are numerous, and by the lengths of filaments seen everywhere in the complex. The column density PDFs have a lognormal shape at low densities and a clearly defined power law at high densities for all sub-regions whose slope is linked to the exponent α of an equivalent spherical density distribution. In particular with α = 2.37, the central sub-region is largly dominated by gravity, caused by individual collapsing dense cores and global collapse of a larger region. The collapse is faster than free-fall (which would lead only to α = 2) and thus requires a more dynamic scenario (external compression, flows). The column density PDFs suggest that the different sub-regions are at different evolutionary stages, especially the central sub-region, which seems to be in a more evolved stage. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.Appendix A is available in electronic form at www.aanda.org</description><identifier>ISSN: 0004-6361</identifier><identifier>EISSN: 1432-0756</identifier><identifier>DOI: 10.1051/0004-6361/201219971</identifier><language>eng</language><publisher>EDP Sciences</publisher><subject>Astrophysics ; Physics ; Sciences of the Universe ; Solar and Stellar Astrophysics</subject><ispartof>Astronomy and astrophysics (Berlin), 2013-06, Vol.554</ispartof><rights>Attribution</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><orcidid>0000-0002-1959-7201 ; 0000-0002-9826-7525 ; 0000-0001-7852-1971 ; 0000-0002-4093-7178 ; 0000-0001-9509-7316 ; 0000-0002-9826-7525 ; 0000-0002-4093-7178 ; 0000-0001-9509-7316 ; 0000-0001-7852-1971 ; 0000-0002-1959-7201</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>230,314,776,780,881,27901,27902</link.rule.ids><backlink>$$Uhttps://hal.science/hal-00838710$$DView record in HAL$$Hfree_for_read</backlink></links><search><creatorcontrib>Russeil, D.</creatorcontrib><creatorcontrib>Schneider, N.</creatorcontrib><creatorcontrib>Anderson, L. D.</creatorcontrib><creatorcontrib>Zavagno, Annie</creatorcontrib><creatorcontrib>Molinari, S.</creatorcontrib><creatorcontrib>Persi, P.</creatorcontrib><creatorcontrib>Bontemps, Sylvain</creatorcontrib><creatorcontrib>Motte, F.</creatorcontrib><creatorcontrib>Ossenkopf, V.</creatorcontrib><creatorcontrib>André, Ph</creatorcontrib><creatorcontrib>Arzoumanian, D.</creatorcontrib><creatorcontrib>Bernard, J.-Ph</creatorcontrib><creatorcontrib>Deharveng, L.</creatorcontrib><creatorcontrib>Didelon, P.</creatorcontrib><creatorcontrib>Di Francesco, J.</creatorcontrib><creatorcontrib>Elia, D.</creatorcontrib><creatorcontrib>Hennemann, M.</creatorcontrib><creatorcontrib>Hill, T.</creatorcontrib><creatorcontrib>Könyves, V.</creatorcontrib><creatorcontrib>Li, J. Z.</creatorcontrib><creatorcontrib>Martin, P. G.</creatorcontrib><creatorcontrib>Nguyen Luong, Q.</creatorcontrib><creatorcontrib>Peretto, N.</creatorcontrib><creatorcontrib>Pezzuto, S.</creatorcontrib><creatorcontrib>Polychroni, D.</creatorcontrib><creatorcontrib>Roussel, Hervé</creatorcontrib><creatorcontrib>Rygl, K. L. J.</creatorcontrib><creatorcontrib>Spinoglio, L.</creatorcontrib><creatorcontrib>Testi, L.</creatorcontrib><creatorcontrib>Tigé, J.</creatorcontrib><creatorcontrib>Vavrek, R.</creatorcontrib><creatorcontrib>Ward-Thompson, D.</creatorcontrib><creatorcontrib>White, G.</creatorcontrib><title>The Herschel view of the massive star-forming region NGC 6334</title><title>Astronomy and astrophysics (Berlin)</title><description>Aims: Fundamental to any theory of high-mass star formation are gravity and turbulence. Their relative importance, which probably changes during cloud evolution, is not known. By investigating the spatial and density structure of the high-mass star-forming complex NGC 6334 we aim to disentangle the contributions of turbulence and gravity. Methods: We used Herschel PACS and SPIRE imaging observations from the HOBYS key programme at wavelengths of 160, 250, 350, and 500 μm to construct dust temperature and column density maps. Using probability distribution functions (PDFs) of the column density determined for the whole complex and for four distinct sub-regions (distinguished on the basis of differences in the column density, temperature, and radiation field), we characterize the density structure of the complex. We investigate the spatial structure using the Δ-variance, which probes the relative amount of structure on different size scales and traces possible energy injection mechanisms into the molecular cloud. Results: The Δ-variance analysis suggests that the significant scales of a few parsec that were found are caused by energy injection due to expanding H ii regions, which are numerous, and by the lengths of filaments seen everywhere in the complex. The column density PDFs have a lognormal shape at low densities and a clearly defined power law at high densities for all sub-regions whose slope is linked to the exponent α of an equivalent spherical density distribution. In particular with α = 2.37, the central sub-region is largly dominated by gravity, caused by individual collapsing dense cores and global collapse of a larger region. The collapse is faster than free-fall (which would lead only to α = 2) and thus requires a more dynamic scenario (external compression, flows). The column density PDFs suggest that the different sub-regions are at different evolutionary stages, especially the central sub-region, which seems to be in a more evolved stage. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.Appendix A is available in electronic form at www.aanda.org</description><subject>Astrophysics</subject><subject>Physics</subject><subject>Sciences of the Universe</subject><subject>Solar and Stellar Astrophysics</subject><issn>0004-6361</issn><issn>1432-0756</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2013</creationdate><recordtype>article</recordtype><recordid>eNqVirsKwjAUQIMoWB9f4JLVIfbepk3bwUGK2kGcupcgaRvpQ5JS8e-tIO5Oh3M4hGwQdggBugDgM8EFuh6gh3Ec4oQ46HOPQRiIKXF-x5wsrL2P6mHEHbLPKkVTZeytUjUdtHrSrqD9GBtprR4Utb00rOhMo9uSGlXqrqXXc0IF5_6KzApZW7X-ckm2p2OWpKySdf4wupHmlXdS5-nhkn8aQMSjEGFA_s_7Bv3SQK0</recordid><startdate>201306</startdate><enddate>201306</enddate><creator>Russeil, D.</creator><creator>Schneider, N.</creator><creator>Anderson, L. D.</creator><creator>Zavagno, Annie</creator><creator>Molinari, S.</creator><creator>Persi, P.</creator><creator>Bontemps, Sylvain</creator><creator>Motte, F.</creator><creator>Ossenkopf, V.</creator><creator>André, Ph</creator><creator>Arzoumanian, D.</creator><creator>Bernard, J.-Ph</creator><creator>Deharveng, L.</creator><creator>Didelon, P.</creator><creator>Di Francesco, J.</creator><creator>Elia, D.</creator><creator>Hennemann, M.</creator><creator>Hill, T.</creator><creator>Könyves, V.</creator><creator>Li, J. Z.</creator><creator>Martin, P. G.</creator><creator>Nguyen Luong, Q.</creator><creator>Peretto, N.</creator><creator>Pezzuto, S.</creator><creator>Polychroni, D.</creator><creator>Roussel, Hervé</creator><creator>Rygl, K. L. J.</creator><creator>Spinoglio, L.</creator><creator>Testi, L.</creator><creator>Tigé, J.</creator><creator>Vavrek, R.</creator><creator>Ward-Thompson, D.</creator><creator>White, G.</creator><general>EDP Sciences</general><scope>1XC</scope><scope>VOOES</scope><orcidid>https://orcid.org/0000-0002-1959-7201</orcidid><orcidid>https://orcid.org/0000-0002-9826-7525</orcidid><orcidid>https://orcid.org/0000-0001-7852-1971</orcidid><orcidid>https://orcid.org/0000-0002-4093-7178</orcidid><orcidid>https://orcid.org/0000-0001-9509-7316</orcidid><orcidid>https://orcid.org/0000-0002-9826-7525</orcidid><orcidid>https://orcid.org/0000-0002-4093-7178</orcidid><orcidid>https://orcid.org/0000-0001-9509-7316</orcidid><orcidid>https://orcid.org/0000-0001-7852-1971</orcidid><orcidid>https://orcid.org/0000-0002-1959-7201</orcidid></search><sort><creationdate>201306</creationdate><title>The Herschel view of the massive star-forming region NGC 6334</title><author>Russeil, D. ; Schneider, N. ; Anderson, L. D. ; Zavagno, Annie ; Molinari, S. ; Persi, P. ; Bontemps, Sylvain ; Motte, F. ; Ossenkopf, V. ; André, Ph ; Arzoumanian, D. ; Bernard, J.-Ph ; Deharveng, L. ; Didelon, P. ; Di Francesco, J. ; Elia, D. ; Hennemann, M. ; Hill, T. ; Könyves, V. ; Li, J. Z. ; Martin, P. G. ; Nguyen Luong, Q. ; Peretto, N. ; Pezzuto, S. ; Polychroni, D. ; Roussel, Hervé ; Rygl, K. L. J. ; Spinoglio, L. ; Testi, L. ; Tigé, J. ; Vavrek, R. ; Ward-Thompson, D. ; White, G.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-hal_primary_oai_HAL_hal_00838710v13</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2013</creationdate><topic>Astrophysics</topic><topic>Physics</topic><topic>Sciences of the Universe</topic><topic>Solar and Stellar Astrophysics</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Russeil, D.</creatorcontrib><creatorcontrib>Schneider, N.</creatorcontrib><creatorcontrib>Anderson, L. D.</creatorcontrib><creatorcontrib>Zavagno, Annie</creatorcontrib><creatorcontrib>Molinari, S.</creatorcontrib><creatorcontrib>Persi, P.</creatorcontrib><creatorcontrib>Bontemps, Sylvain</creatorcontrib><creatorcontrib>Motte, F.</creatorcontrib><creatorcontrib>Ossenkopf, V.</creatorcontrib><creatorcontrib>André, Ph</creatorcontrib><creatorcontrib>Arzoumanian, D.</creatorcontrib><creatorcontrib>Bernard, J.-Ph</creatorcontrib><creatorcontrib>Deharveng, L.</creatorcontrib><creatorcontrib>Didelon, P.</creatorcontrib><creatorcontrib>Di Francesco, J.</creatorcontrib><creatorcontrib>Elia, D.</creatorcontrib><creatorcontrib>Hennemann, M.</creatorcontrib><creatorcontrib>Hill, T.</creatorcontrib><creatorcontrib>Könyves, V.</creatorcontrib><creatorcontrib>Li, J. Z.</creatorcontrib><creatorcontrib>Martin, P. G.</creatorcontrib><creatorcontrib>Nguyen Luong, Q.</creatorcontrib><creatorcontrib>Peretto, N.</creatorcontrib><creatorcontrib>Pezzuto, S.</creatorcontrib><creatorcontrib>Polychroni, D.</creatorcontrib><creatorcontrib>Roussel, Hervé</creatorcontrib><creatorcontrib>Rygl, K. L. J.</creatorcontrib><creatorcontrib>Spinoglio, L.</creatorcontrib><creatorcontrib>Testi, L.</creatorcontrib><creatorcontrib>Tigé, J.</creatorcontrib><creatorcontrib>Vavrek, R.</creatorcontrib><creatorcontrib>Ward-Thompson, D.</creatorcontrib><creatorcontrib>White, G.</creatorcontrib><collection>Hyper Article en Ligne (HAL)</collection><collection>Hyper Article en Ligne (HAL) (Open Access)</collection><jtitle>Astronomy and astrophysics (Berlin)</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Russeil, D.</au><au>Schneider, N.</au><au>Anderson, L. D.</au><au>Zavagno, Annie</au><au>Molinari, S.</au><au>Persi, P.</au><au>Bontemps, Sylvain</au><au>Motte, F.</au><au>Ossenkopf, V.</au><au>André, Ph</au><au>Arzoumanian, D.</au><au>Bernard, J.-Ph</au><au>Deharveng, L.</au><au>Didelon, P.</au><au>Di Francesco, J.</au><au>Elia, D.</au><au>Hennemann, M.</au><au>Hill, T.</au><au>Könyves, V.</au><au>Li, J. Z.</au><au>Martin, P. G.</au><au>Nguyen Luong, Q.</au><au>Peretto, N.</au><au>Pezzuto, S.</au><au>Polychroni, D.</au><au>Roussel, Hervé</au><au>Rygl, K. L. J.</au><au>Spinoglio, L.</au><au>Testi, L.</au><au>Tigé, J.</au><au>Vavrek, R.</au><au>Ward-Thompson, D.</au><au>White, G.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>The Herschel view of the massive star-forming region NGC 6334</atitle><jtitle>Astronomy and astrophysics (Berlin)</jtitle><date>2013-06</date><risdate>2013</risdate><volume>554</volume><issn>0004-6361</issn><eissn>1432-0756</eissn><abstract>Aims: Fundamental to any theory of high-mass star formation are gravity and turbulence. Their relative importance, which probably changes during cloud evolution, is not known. By investigating the spatial and density structure of the high-mass star-forming complex NGC 6334 we aim to disentangle the contributions of turbulence and gravity. Methods: We used Herschel PACS and SPIRE imaging observations from the HOBYS key programme at wavelengths of 160, 250, 350, and 500 μm to construct dust temperature and column density maps. Using probability distribution functions (PDFs) of the column density determined for the whole complex and for four distinct sub-regions (distinguished on the basis of differences in the column density, temperature, and radiation field), we characterize the density structure of the complex. We investigate the spatial structure using the Δ-variance, which probes the relative amount of structure on different size scales and traces possible energy injection mechanisms into the molecular cloud. Results: The Δ-variance analysis suggests that the significant scales of a few parsec that were found are caused by energy injection due to expanding H ii regions, which are numerous, and by the lengths of filaments seen everywhere in the complex. The column density PDFs have a lognormal shape at low densities and a clearly defined power law at high densities for all sub-regions whose slope is linked to the exponent α of an equivalent spherical density distribution. In particular with α = 2.37, the central sub-region is largly dominated by gravity, caused by individual collapsing dense cores and global collapse of a larger region. The collapse is faster than free-fall (which would lead only to α = 2) and thus requires a more dynamic scenario (external compression, flows). The column density PDFs suggest that the different sub-regions are at different evolutionary stages, especially the central sub-region, which seems to be in a more evolved stage. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.Appendix A is available in electronic form at www.aanda.org</abstract><pub>EDP Sciences</pub><doi>10.1051/0004-6361/201219971</doi><orcidid>https://orcid.org/0000-0002-1959-7201</orcidid><orcidid>https://orcid.org/0000-0002-9826-7525</orcidid><orcidid>https://orcid.org/0000-0001-7852-1971</orcidid><orcidid>https://orcid.org/0000-0002-4093-7178</orcidid><orcidid>https://orcid.org/0000-0001-9509-7316</orcidid><orcidid>https://orcid.org/0000-0002-9826-7525</orcidid><orcidid>https://orcid.org/0000-0002-4093-7178</orcidid><orcidid>https://orcid.org/0000-0001-9509-7316</orcidid><orcidid>https://orcid.org/0000-0001-7852-1971</orcidid><orcidid>https://orcid.org/0000-0002-1959-7201</orcidid><oa>free_for_read</oa></addata></record>
fulltext fulltext
identifier ISSN: 0004-6361
ispartof Astronomy and astrophysics (Berlin), 2013-06, Vol.554
issn 0004-6361
1432-0756
language eng
recordid cdi_hal_primary_oai_HAL_hal_00838710v1
source EZB Electronic Journals Library
subjects Astrophysics
Physics
Sciences of the Universe
Solar and Stellar Astrophysics
title The Herschel view of the massive star-forming region NGC 6334
url http://sfxeu10.hosted.exlibrisgroup.com/loughborough?ctx_ver=Z39.88-2004&ctx_enc=info:ofi/enc:UTF-8&ctx_tim=2025-02-18T11%3A27%3A25IST&url_ver=Z39.88-2004&url_ctx_fmt=infofi/fmt:kev:mtx:ctx&rfr_id=info:sid/primo.exlibrisgroup.com:primo3-Article-hal&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.genre=article&rft.atitle=The%20Herschel%20view%20of%20the%20massive%20star-forming%20region%20NGC%206334&rft.jtitle=Astronomy%20and%20astrophysics%20(Berlin)&rft.au=Russeil,%20D.&rft.date=2013-06&rft.volume=554&rft.issn=0004-6361&rft.eissn=1432-0756&rft_id=info:doi/10.1051/0004-6361/201219971&rft_dat=%3Chal%3Eoai_HAL_hal_00838710v1%3C/hal%3E%3Cgrp_id%3Ecdi_FETCH-hal_primary_oai_HAL_hal_00838710v13%3C/grp_id%3E%3Coa%3E%3C/oa%3E%3Curl%3E%3C/url%3E&rft_id=info:oai/&rft_id=info:pmid/&rfr_iscdi=true