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Treviño-Morales SP, Fuente A, Sánchez-Monge Á, Kainulainen J, Didelon P, Suri S, Schneider N, Ballesteros-Paredes J, Lee YN, Hennebelle P, Pilleri P, González-García M, Kramer C, García-Burillo S, Luna A, Goicoechea JR, Tremblin P, Geen S. Dynamics of cluster-forming hub-filament systems: The case of the high-mass star-forming complex Monoceros R2. ASTRONOMY AND ASTROPHYSICS 2019; 629:A81. [PMID: 31673163 PMCID: PMC6823053 DOI: 10.1051/0004-6361/201935260] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/10/2023]
Abstract
CONTEXT High-mass stars and star clusters commonly form within hub-filament systems. Monoceros R2 (hereafter Mon R2), at a distance of 830 pc, harbors one of the closest such systems, making it an excellent target for case studies. AIMS We investigate the morphology, stability and dynamical properties of the Mon R2 hub-filament system. METHODS We employ observations of the 13CO and C18O 1→0 and 2→1 lines obtained with the IRAM-30m telescope. We also use H2 column density maps derived from Herschel dust emission observations. RESULTS We identified the filamentary network in Mon R2 with the DisPerSE algorithm and characterized the individual filaments as either main (converging into the hub) or secondary (converging to a main filament) filaments. The main filaments have line masses of 30-100 M ⊙ pc-1 and show signs of fragmentation, while the secondary filaments have line masses of 12-60 M ⊙ pc-1 and show fragmentation only sporadically. In the context of Ostriker's hydrostatic filament model, the main filaments are thermally supercritical. If non-thermal motions are included, most of them are trans-critical. Most of the secondary filaments are roughly transcritical regardless of whether non-thermal motions are included or not. From the morphology and kinematics of the main filaments, we estimate a mass accretion rate of 10-4-10-3 M ⊙ yr-1 into the central hub. The secondary filaments accrete into the main filaments with a rate of 0.1-0.4×10-4 M ⊙ yr-1. The main filaments extend into the central hub. Their velocity gradients increase towards the hub, suggesting acceleration of the gas.We estimate that with the observed infall velocity, the mass-doubling time of the hub is ~ 2:5 Myr, ten times larger than the free-fall time, suggesting a dynamically old region. These timescales are comparable with the chemical age of the Hii region. Inside the hub, the main filaments show a ring- or a spiral-like morphology that exhibits rotation and infall motions. One possible explanation for the morphology is that gas is falling into the central cluster following a spiral-like pattern.
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Affiliation(s)
- S P Treviño-Morales
- Chalmers University of Technology, Department of Space, Earth and Environment, SE-412 93 Gothenburg, Sweden
| | - A Fuente
- Observatorio Astronómico Nacional, Apdo. 112, 28803 Alcalá de Henares Madrid, Spain
| | - Á Sánchez-Monge
- I. Physikalisches Institut, Universität zu Köln, Zülpicher Str. 77, 50937 Köln, Germany
| | - J Kainulainen
- Chalmers University of Technology, Department of Space, Earth and Environment, SE-412 93 Gothenburg, Sweden
- Max-Planck-Institute for Astronomy, Königstuhl 17, 69117 Heidelberg, Germany
| | - P Didelon
- Laboratoire AIM, Paris-Saclay, CEA/IRFU/SAp - CNRS - Université Paris Diderot, 91191 Gif-sur-Yvette Cedex, France
| | - S Suri
- I. Physikalisches Institut, Universität zu Köln, Zülpicher Str. 77, 50937 Köln, Germany
- Max-Planck-Institute for Astronomy, Königstuhl 17, 69117 Heidelberg, Germany
| | - N Schneider
- I. Physikalisches Institut, Universität zu Köln, Zülpicher Str. 77, 50937 Köln, Germany
| | - J Ballesteros-Paredes
- Instituto de Radioastronomía y Astrofísica, Universidad Nacional Autónoma de México, P.O. Box 3-72, 58090 Morelia, Mexico
| | - Y-N Lee
- Institut de Physique du Globe de Paris, Sorbonne Paris Cité, Université Paris Diderot, UMR 7154 CNRS, 75005 Paris, France
| | - P Hennebelle
- Laboratoire AIM, Paris-Saclay, CEA/IRFU/SAp - CNRS - Université Paris Diderot, 91191 Gif-sur-Yvette Cedex, France
| | - P Pilleri
- IRAP, Université de Toulouse, CNRS, UPS, CNES, 9 Av. colonel Roche, BP 44346, 31028 Toulouse Cedex 4, France
| | - M González-García
- Instituto de Astrofísica de Andalucía, IAA-CSIC, Glorieta de la Astronomía s/n, 18008 Granada, Spain
| | - C Kramer
- Institut de Radioastronomie Millimétrique (IRAM), 300 rue de la Piscine, 38406 Saint Martin d'Hères, France
| | - S García-Burillo
- Observatorio Astronómico Nacional, Apdo. 112, 28803 Alcalá de Henares Madrid, Spain
| | - A Luna
- Instituto Nacional de Astrofísica, Óptica y Electrónica, Luis Enrique Erro #1, 72840 Tonantzintla, Puebla, Mexico
| | - J R Goicoechea
- Instituto de Física Fundamental (CSIC). Calle Serrano 121, E-28006, Madrid, Spain
| | - P Tremblin
- Laboratoire AIM, Paris-Saclay, CEA/IRFU/SAp - CNRS - Université Paris Diderot, 91191 Gif-sur-Yvette Cedex, France
| | - S Geen
- Zentrum für Astronomie, Institut für Theoretische Astrophysik, Universität Heidelberg, Albert-Ueberle-Str. 2, 69120 Heidelberg, Germany
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Rivière-Marichalar P, Fuente A, Goicoechea JR, Pety J, Le Gal R, Gratier P, Guzmán V, Roueff E, Loison JC, Wakelam V, Gerin M. Abundances of sulphur molecules in the Horsehead nebula First NS + detection in a photodissociation region. ASTRONOMY AND ASTROPHYSICS 2019; 628:A16. [PMID: 31511745 PMCID: PMC6739222 DOI: 10.1051/0004-6361/201935354] [Citation(s) in RCA: 8] [Impact Index Per Article: 1.6] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/10/2023]
Abstract
CONTEXT Sulphur is one of the most abundant elements in the Universe (S/H∼1.3×10 -5 ) and plays a crucial role in biological systems on Earth. The understanding of its chemistry is therefore of major importance. AIMS Our goal is to complete the inventory of S-bearing molecules and their abundances in the prototypical photodissociation region (PDR) the Horsehead nebula to gain insight into sulphur chemistry in UV irradiated regions. Based on the WHISPER (Wide-band High-resolution Iram-30m Surveys at two positions with Emir Receivers) millimeter (mm) line survey, our goal is to provide an improved and more accurate description of sulphur species and their abundances towards the core and PDR positions in the Horsehead. METHODS The Monte Carlo Markov Chain (MCMC) methodology and the molecular excitation and radiative transfer code RADEX were used to explore the parameter space and determine physical conditions and beam-averaged molecular abundances. RESULTS A total of 13 S-bearing species (CS, SO, SO2, OCS, H2CS - both ortho and para - HDCS, C2S, HCS+, SO+, H2S, S2H, NS and NS+) have been detected in the two targeted positions. This is the first detection of SO+ in the Horsehead and the first detection of NS+ in any PDR. We find a differentiated chemical behaviour between C-S and O-S bearing species within the nebula. The C-S bearing species C2S and o-H2CS present fractional abundances a factor of > two higher in the core than in the PDR. In contrast, the O-S bearing molecules SO, SO2, and OCS present similar abundances towards both positions. A few molecules, SO+, NS, and NS+, are more abundant towards the PDR than towards the core, and could be considered as PDR tracers. CONCLUSIONS This is the first complete study of S-bearing species towards a PDR. Our study shows that CS, SO, and H2S are the most abundant S-bearing molecules in the PDR with abundances of ∼ a few 10-9. We recall that SH, SH+, S, and S+ are not observable at the wavelengths covered by the WHISPER survey. At the spatial scale of our observations, the total abundance of S atoms locked in the detected species is < 10-8, only ∼0.1% of the cosmic sulphur abundance.
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Affiliation(s)
- P Rivière-Marichalar
- Instituto de Física Fundamental (CSIC), Calle Serrano 121, 28006 Madrid, Spain
- Observatorio Astronómico Nacional (OAN,IGN), Apdo 112, E-28803 Alcalá de Henares, Spain
| | - A Fuente
- Observatorio Astronómico Nacional (OAN,IGN), Apdo 112, E-28803 Alcalá de Henares, Spain
| | - J R Goicoechea
- Instituto de Física Fundamental (CSIC), Calle Serrano 121, 28006 Madrid, Spain
| | - J Pety
- Institut de Radioastronomie Millimétrique (IRAM), 300 rue de la Piscine, 38406 Saint Martin d'Hères, France
- LERMA, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Universités, UPMC Univ. Paris 06, Ecole Normale Supérieure, F-75005 Paris, France
| | - R Le Gal
- Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138, USA
| | - P Gratier
- Laboratoire d'Astrophysique de Bordeaux, Univ. Bordeaux, CNRS, B18N, allée Geoffroy Saint-Hilaire, 33615 Pessac, France
| | - V Guzmán
- Instituto de Astrofísica, Pontificia Universidad Católica de Chile, Av. Vicunña Mackenna, 4860, 7820436, Macul, Santiago, Chile
| | - E Roueff
- LERMA, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Universités, UPMC Univ. Paris 06, F-92190 Meudon, France
| | - J C Loison
- Institut des Sciences Moléculaires de Bordeaux (ISM), CNRS, Univ. Bordeaux, 351 cours de la Libération, 33400, Talence, France
| | - V Wakelam
- Laboratoire d'Astrophysique de Bordeaux, Univ. Bordeaux, CNRS, B18N, allée Geoffroy Saint-Hilaire, 33615 Pessac, France
| | - M Gerin
- LERMA, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Universités, UPMC Univ. Paris 06, Ecole Normale Supérieure, F-75005 Paris, France
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Rayner TSM, Griffin MJ, Schneider N, Motte F, Kӧnyves V, André P, Di Francesco J, Didelon P, Pattle K, Ward-Thompson D, Anderson LD, Benedettini M, Bernard JP, Bontemps S, Elia D, Fuente A, Hennemann M, Hill T, Kirk J, Marsh K, Men’shchikov A, Nguyen Luong Q, Peretto N, Pezzuto S, Rivera-Ingraham A, Roy A, Rygl K, Sánchez-Monge Á, Spinoglio L, Tigé J, Treviño-Morales SP, White GJ. Far-infrared observations of a massive cluster forming in the Monoceros R2 filament hub ⋆. ASTRONOMY AND ASTROPHYSICS 2017; 607:A22. [PMID: 31844331 PMCID: PMC6914369 DOI: 10.1051/0004-6361/201630039] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/10/2023]
Abstract
We present far-infrared observations of Monoceros R2 (a giant molecular cloud at approximately 830 pc distance, containing several sites of active star formation), as observed at 70 μm, 160 μm, 250 μm, 350 μm, and 500 μm by the Photodetector Array Camera and Spectrometer (PACS) and Spectral and Photometric Imaging Receiver (SPIRE) instruments on the Herschel Space Observatory as part of the Herschel imaging survey of OB young stellar objects (HOBYS) Key programme. The Herschel data are complemented by SCUBA-2 data in the submillimetre range, and WISE and Spitzer data in the mid-infrared. In addition, C18O data from the IRAM 30-m Telescope are presented, and used for kinematic information. Sources were extracted from the maps with getsources, and from the fluxes measured, spectral energy distributions were constructed, allowing measurements of source mass and dust temperature. Of 177 Herschel sources robustly detected in the region (a detection with high signal-to-noise and low axis ratio at multiple wavelengths), including protostars and starless cores, 29 are found in a filamentary hub at the centre of the region (a little over 1% of the observed area). These objects are on average smaller, more massive, and more luminous than those in the surrounding regions (which together suggest that they are at a later stage of evolution), a result that cannot be explained entirely by selection effects. These results suggest a picture in which the hub may have begun star formation at a point significantly earlier than the outer regions, possibly forming as a result of feedback from earlier star formation. Furthermore, the hub may be sustaining its star formation by accreting material from the surrounding filaments.
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Affiliation(s)
- T. S. M. Rayner
- Cardiff School of Physics and Astronomy, Cardiff University,
Queen’s Buildings, The Parade, Cardiff, Wales, CF24 3AA, UK
| | - M. J. Griffin
- Cardiff School of Physics and Astronomy, Cardiff University,
Queen’s Buildings, The Parade, Cardiff, Wales, CF24 3AA, UK
| | - N. Schneider
- I. Physik. Institut, University of Cologne, 50937 Cologne,
Germany
- Laboratoire d’Astrophysique de Bordeaux, Univ. Bordeaux,
CNRS, B18N, allée G. Saint-Hilaire, 33615 Pessac, France
| | - F. Motte
- Université Grenoble Alpes, CNRS, Institut de Planetologie et
d’Astrophysique de Grenoble, 38000 Grenoble, France
- Laboratoire AIM, CEA/IRFU – CNRS/INSU –
Université Paris Diderot, CEA-Saclay, 91191 Gif-sur-Yvette Cedex,
France
| | - V. Kӧnyves
- Laboratoire AIM, CEA/IRFU – CNRS/INSU –
Université Paris Diderot, CEA-Saclay, 91191 Gif-sur-Yvette Cedex,
France
| | - P. André
- Laboratoire AIM, CEA/IRFU – CNRS/INSU –
Université Paris Diderot, CEA-Saclay, 91191 Gif-sur-Yvette Cedex,
France
| | | | - P. Didelon
- Laboratoire AIM, CEA/IRFU – CNRS/INSU –
Université Paris Diderot, CEA-Saclay, 91191 Gif-sur-Yvette Cedex,
France
| | - K. Pattle
- Jeremiah Horrocks Institute, University of Central Lancashire,
Preston PR1 2HE, UK
| | - D. Ward-Thompson
- Jeremiah Horrocks Institute, University of Central Lancashire,
Preston PR1 2HE, UK
| | - L. D. Anderson
- Department of Physics and Astronomy, West Virginia University,
Morgantown, WV 26506, USA
| | - M. Benedettini
- INAF – Istituto di Astrofisica e Planetologia Spaziali, via
Fosso del Cavaliere 100, I-00133 Roma, Italy
| | - J-P. Bernard
- Université de Toulouse, UPS-OMP, IRAP, Toulouse,
France
| | - S. Bontemps
- Laboratoire d’Astrophysique de Bordeaux, Univ. Bordeaux,
CNRS, B18N, allée G. Saint-Hilaire, 33615 Pessac, France
| | - D. Elia
- INAF – Istituto di Astrofisica e Planetologia Spaziali, via
Fosso del Cavaliere 100, I-00133 Roma, Italy
| | - A. Fuente
- Observatorio Astronómico Nacional (OAN), Apdo 112, E-28803
Alcalá de Henares, Madrid, Spain
| | - M. Hennemann
- Laboratoire AIM, CEA/IRFU – CNRS/INSU –
Université Paris Diderot, CEA-Saclay, 91191 Gif-sur-Yvette Cedex,
France
| | - T. Hill
- Laboratoire AIM, CEA/IRFU – CNRS/INSU –
Université Paris Diderot, CEA-Saclay, 91191 Gif-sur-Yvette Cedex,
France
- Joint ALMA Observatory, 3107 Alonso de Cordova, Vitacura, Santiago,
Chile
| | - J. Kirk
- Jeremiah Horrocks Institute, University of Central Lancashire,
Preston PR1 2HE, UK
| | - K. Marsh
- Cardiff School of Physics and Astronomy, Cardiff University,
Queen’s Buildings, The Parade, Cardiff, Wales, CF24 3AA, UK
| | - A. Men’shchikov
- Laboratoire AIM, CEA/IRFU – CNRS/INSU –
Université Paris Diderot, CEA-Saclay, 91191 Gif-sur-Yvette Cedex,
France
| | - Q. Nguyen Luong
- Korea Astronomy and Space Science Institute, 776 Daedeokdae-ro,
Yuseong-gu, Daejeon, 305-348, Republic of Korea
- National Astronomical Observatory of Japan, Chile Observatory,
2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
| | - N. Peretto
- Cardiff School of Physics and Astronomy, Cardiff University,
Queen’s Buildings, The Parade, Cardiff, Wales, CF24 3AA, UK
| | - S. Pezzuto
- INAF – Istituto di Astrofisica e Planetologia Spaziali, via
Fosso del Cavaliere 100, I-00133 Roma, Italy
| | | | - A. Roy
- Laboratoire AIM, CEA/IRFU – CNRS/INSU –
Université Paris Diderot, CEA-Saclay, 91191 Gif-sur-Yvette Cedex,
France
| | - K. Rygl
- INAF – Istituto di Radioastronomia, Via Gobetti 101, I-40129
Bologna, Italy
| | - Á. Sánchez-Monge
- I. Physik. Institut, University of Cologne, 50937 Cologne,
Germany
| | - L. Spinoglio
- INAF – Istituto di Astrofisica e Planetologia Spaziali, via
Fosso del Cavaliere 100, I-00133 Roma, Italy
| | - J. Tigé
- Aix-Marseille Université, CNRS, LAM (Laboratoire
d’Astrophysique de Marseille) UMR 7326, 13388 Marseille, France
| | - S. P. Treviño-Morales
- Instituto de Ciencia de Materiales de Madrid (ICMM-CSIC), Sor Juana
Inés de la Cruz 3, E-28049 Cantoblanco, Madrid, Spain
| | - G. J. White
- The Rutherford Appleton Laboratory, Chilton, Didcot OX11 0NL,
UK
- Department of Physics and Astronomy, The Open University, Milton
Keynes, UK
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