Galactic star formation with NIKA2 (GASTON): Filament convergence and its link to star formation
In the past decade filaments have been recognised as a major structural element of the interstellar medium, the densest of these filaments hosting the formation of most stars. In some star-forming molecular clouds converging networks of filaments, also known as hub filament systems, can be found. Th...
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EDP Sciences
2022-01-01
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| Series: | EPJ Web of Conferences |
| Online Access: | https://www.epj-conferences.org/articles/epjconf/pdf/2022/01/epjconf_mmUniverse2021_00037.pdf |
| _version_ | 1798014307667017728 |
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| author | Peretto N. Adam R. Ade P. Ajeddig H. André P. Artis E. Aussel H. Bacmann A. Beelen A. Benoît A. Berta S. Bing L. Bourrion O. Calvo M. Catalano A. De Petris M. Désert F.-X. Doyle S. Driessen E. F. C. Gomez A. Goupy J. Kéruzoré F. Kramer C. Ladjelate B. Lagache G. Leclercq S. Lestrade J.-F. Macías-Pérez J.-F. Maury A. Mauskopf P. Mayet F. Monfardini A. Muñoz-Echeverría M. Perotto L. Pisano G. Ponthieu N. Revéret V. Rigby A. Ristorcelli I. Ritacco A. Romero C. Roussel H. Ruppin F. Schuster K. Shu S. Sievers A. Tucker C. Zylka R. |
| author_facet | Peretto N. Adam R. Ade P. Ajeddig H. André P. Artis E. Aussel H. Bacmann A. Beelen A. Benoît A. Berta S. Bing L. Bourrion O. Calvo M. Catalano A. De Petris M. Désert F.-X. Doyle S. Driessen E. F. C. Gomez A. Goupy J. Kéruzoré F. Kramer C. Ladjelate B. Lagache G. Leclercq S. Lestrade J.-F. Macías-Pérez J.-F. Maury A. Mauskopf P. Mayet F. Monfardini A. Muñoz-Echeverría M. Perotto L. Pisano G. Ponthieu N. Revéret V. Rigby A. Ristorcelli I. Ritacco A. Romero C. Roussel H. Ruppin F. Schuster K. Shu S. Sievers A. Tucker C. Zylka R. |
| author_sort | Peretto N. |
| collection | DOAJ |
| description | In the past decade filaments have been recognised as a major structural element of the interstellar medium, the densest of these filaments hosting the formation of most stars. In some star-forming molecular clouds converging networks of filaments, also known as hub filament systems, can be found. These hubs are believed to be preferentially associated to massive star formation. As of today, there are no metrics that allow the systematic quantification of a filament network convergence. Here, we used the IRAM 30m NIKA2 observations of the Galactic plane from the GASTON large programme to systematically identify filaments and produce a filament convergence parameter map. We use such a map to show that: i. hub filaments represent a small fraction of the global filament population; ii. hubs host, in proportion, more massive and more luminous compact sources that non-hubs; iii. hub-hosting clumps are more evolved that non-hubs; iv. no discontinuities are observed in the properties of compact sources as a function of convergence parameter. We propose that the rapid global collapse of clumps is responsible for (re)organising filament networks into hubs and, in parallel, enhancing the mass growth of compact sources. |
| first_indexed | 2024-04-11T15:16:29Z |
| format | Article |
| id | doaj.art-e28fb8e29da643658984d25c08d73e55 |
| institution | Directory Open Access Journal |
| issn | 2100-014X |
| language | English |
| last_indexed | 2024-04-11T15:16:29Z |
| publishDate | 2022-01-01 |
| publisher | EDP Sciences |
| record_format | Article |
| series | EPJ Web of Conferences |
| spelling | doaj.art-e28fb8e29da643658984d25c08d73e552022-12-22T04:16:29ZengEDP SciencesEPJ Web of Conferences2100-014X2022-01-012570003710.1051/epjconf/202225700037epjconf_mmUniverse2021_00037Galactic star formation with NIKA2 (GASTON): Filament convergence and its link to star formationPeretto N.0Adam R.1Ade P.2Ajeddig H.3André P.4Artis E.5Aussel H.6Bacmann A.7Beelen A.8Benoît A.9Berta S.10Bing L.11Bourrion O.12Calvo M.13Catalano A.14De Petris M.15Désert F.-X.16Doyle S.17Driessen E. F. C.18Gomez A.19Goupy J.20Kéruzoré F.21Kramer C.22Ladjelate B.23Lagache G.24Leclercq S.25Lestrade J.-F.26Macías-Pérez J.-F.27Maury A.28Mauskopf P.29Mayet F.30Monfardini A.31Muñoz-Echeverría M.32Perotto L.33Pisano G.34Ponthieu N.35Revéret V.36Rigby A.37Ristorcelli I.38Ritacco A.39Romero C.40Roussel H.41Ruppin F.42Schuster K.43Shu S.44Sievers A.45Tucker C.46Zylka R.47School of Physics and Astronomy, Cardiff University, Queen’s Buildings, The ParadeLLR (Laboratoire Leprince-Ringuet), CNRS, École Polytechnique, Institut Polytechnique de ParisSchool of Physics and Astronomy, Cardiff University, Queen’s Buildings, The ParadeAIM, CEA, CNRS, Université Paris-Saclay, Université Paris Diderot, Sorbonne Paris CitéAIM, CEA, CNRS, Université Paris-Saclay, Université Paris Diderot, Sorbonne Paris CitéUniv. Grenoble Alpes, CNRS, Grenoble INP, LPSC-IN2P3AIM, CEA, CNRS, Université Paris-Saclay, Université Paris Diderot, Sorbonne Paris CitéUniv. Grenoble Alpes, CNRS, IPAGInstitut d’Astrophysique Spatiale (IAS), CNRS, Université Paris SudInstitut Néel, CNRS, Université Grenoble AlpesInstitut de RadioAstronomie Millimétrique (IRAM)Aix Marseille Univ, CNRS, CNES, LAM (Laboratoire d’Astrophysique de Marseille)Univ. Grenoble Alpes, CNRS, Grenoble INP, LPSC-IN2P3Institut Néel, CNRS, Université Grenoble AlpesUniv. Grenoble Alpes, CNRS, Grenoble INP, LPSC-IN2P3Dipartimento di Fisica, Sapienza Università di RomaUniv. Grenoble Alpes, CNRS, IPAGSchool of Physics and Astronomy, Cardiff University, Queen’s Buildings, The ParadeInstitut de RadioAstronomie Millimétrique (IRAM)Centro de Astrobiología (CSIC-INTA), Torrejón de ArdozInstitut Néel, CNRS, Université Grenoble AlpesUniv. Grenoble Alpes, CNRS, Grenoble INP, LPSC-IN2P3Instituto de Radioastronomía Milimétrica (IRAM)Instituto de Radioastronomía Milimétrica (IRAM)Aix Marseille Univ, CNRS, CNES, LAM (Laboratoire d’Astrophysique de Marseille)Institut de RadioAstronomie Millimétrique (IRAM)LERMA, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Université, UPMCUniv. Grenoble Alpes, CNRS, Grenoble INP, LPSC-IN2P3AIM, CEA, CNRS, Université Paris-Saclay, Université Paris Diderot, Sorbonne Paris CitéSchool of Physics and Astronomy, Cardiff University, Queen’s Buildings, The ParadeUniv. Grenoble Alpes, CNRS, Grenoble INP, LPSC-IN2P3Institut Néel, CNRS, Université Grenoble AlpesUniv. Grenoble Alpes, CNRS, Grenoble INP, LPSC-IN2P3Univ. Grenoble Alpes, CNRS, Grenoble INP, LPSC-IN2P3School of Physics and Astronomy, Cardiff University, Queen’s Buildings, The ParadeUniv. Grenoble Alpes, CNRS, IPAGAIM, CEA, CNRS, Université Paris-Saclay, Université Paris Diderot, Sorbonne Paris CitéSchool of Physics and Astronomy, Cardiff University, Queen’s Buildings, The ParadeUniv. Toulouse, CNRS, IRAPInstitut d’Astrophysique Spatiale (IAS), CNRS, Université Paris SudDepartment of Physics and Astronomy, University of PennsylvaniaInstitut d’Astrophysique de Paris, Sorbonne Université, CNRS (UMR7095)Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of TechnologyInstitut de RadioAstronomie Millimétrique (IRAM)CaltechInstituto de Radioastronomía Milimétrica (IRAM)School of Physics and Astronomy, Cardiff University, Queen’s Buildings, The ParadeInstitut de RadioAstronomie Millimétrique (IRAM)In the past decade filaments have been recognised as a major structural element of the interstellar medium, the densest of these filaments hosting the formation of most stars. In some star-forming molecular clouds converging networks of filaments, also known as hub filament systems, can be found. These hubs are believed to be preferentially associated to massive star formation. As of today, there are no metrics that allow the systematic quantification of a filament network convergence. Here, we used the IRAM 30m NIKA2 observations of the Galactic plane from the GASTON large programme to systematically identify filaments and produce a filament convergence parameter map. We use such a map to show that: i. hub filaments represent a small fraction of the global filament population; ii. hubs host, in proportion, more massive and more luminous compact sources that non-hubs; iii. hub-hosting clumps are more evolved that non-hubs; iv. no discontinuities are observed in the properties of compact sources as a function of convergence parameter. We propose that the rapid global collapse of clumps is responsible for (re)organising filament networks into hubs and, in parallel, enhancing the mass growth of compact sources.https://www.epj-conferences.org/articles/epjconf/pdf/2022/01/epjconf_mmUniverse2021_00037.pdf |
| spellingShingle | Peretto N. Adam R. Ade P. Ajeddig H. André P. Artis E. Aussel H. Bacmann A. Beelen A. Benoît A. Berta S. Bing L. Bourrion O. Calvo M. Catalano A. De Petris M. Désert F.-X. Doyle S. Driessen E. F. C. Gomez A. Goupy J. Kéruzoré F. Kramer C. Ladjelate B. Lagache G. Leclercq S. Lestrade J.-F. Macías-Pérez J.-F. Maury A. Mauskopf P. Mayet F. Monfardini A. Muñoz-Echeverría M. Perotto L. Pisano G. Ponthieu N. Revéret V. Rigby A. Ristorcelli I. Ritacco A. Romero C. Roussel H. Ruppin F. Schuster K. Shu S. Sievers A. Tucker C. Zylka R. Galactic star formation with NIKA2 (GASTON): Filament convergence and its link to star formation EPJ Web of Conferences |
| title | Galactic star formation with NIKA2 (GASTON): Filament convergence and its link to star formation |
| title_full | Galactic star formation with NIKA2 (GASTON): Filament convergence and its link to star formation |
| title_fullStr | Galactic star formation with NIKA2 (GASTON): Filament convergence and its link to star formation |
| title_full_unstemmed | Galactic star formation with NIKA2 (GASTON): Filament convergence and its link to star formation |
| title_short | Galactic star formation with NIKA2 (GASTON): Filament convergence and its link to star formation |
| title_sort | galactic star formation with nika2 gaston filament convergence and its link to star formation |
| url | https://www.epj-conferences.org/articles/epjconf/pdf/2022/01/epjconf_mmUniverse2021_00037.pdf |
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