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Navarro-Almaida D, Le Gal R, Fuente A, Rivière-Marichalar P, Wakelam V, Cazaux S, Caselli P, Laas JC, Alonso-Albi T, Loison JC, Gerin M, Kramer C, Roueff E, Bachiller R, Commerçon B, Friesen R, García-Burillo S, Goicoechea JR, Giuliano BM, Jiménez-Serra I, Kirk JM, Lattanzi V, Malinen J, Marcelino N, Martín-Domènech R, Muñoz Caro GM, Pineda J, Tercero B, Treviño-Morales SP, Roncero O, Hacar A, Tafalla M, Ward-Thompson D. Gas phase Elemental abundances in Molecular cloudS (GEMS) II. On the quest for the sulphur reservoir in molecular clouds: the H 2S case. Astron Astrophys 2020; 637:A39. [PMID: 32565548 PMCID: PMC7305024 DOI: 10.1051/0004-6361/201937180] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/11/2023]
Abstract
CONTEXT Sulphur is one of the most abundant elements in the Universe. Surprisingly, sulphuretted molecules are not as abundant as expected in the interstellar medium and the identity of the main sulphur reservoir is still an open question. AIMS Our goal is to investigate the H2S chemistry in dark clouds, as this stable molecule is a potential sulphur reservoir. METHODS Using millimeter observations of CS, SO, H2S, and their isotopologues, we determine the physical conditions and H2S abundances along the cores TMC 1-C, TMC 1-CP, and Barnard 1b. The gas-grain model Nautilus is used to model the sulphur chemistry and explore the impact of photo-desorption and chemical desorption on the H2S abundance. RESULTS Our modeling shows that chemical desorption is the main source of gas-phase H2S in dark cores. The measured H2S abundance can only be fitted if we assume that the chemical desorption rate decreases by more than a factor of 10 when n H > 2 × 104. This change in the desorption rate is consistent with the formation of thick H2O and CO ice mantles on grain surfaces. The observed SO and H2S abundances are in good agreement with our predictions adopting an undepleted value of the sulphur abundance. However, the CS abundance is overestimated by a factor of 5 - 10. Along the three cores, atomic S is predicted to be the main sulphur reservoir. CONCLUSIONS The gaseous H2S abundance is well reproduced, assuming undepleted sulphur abundance and chemical desorption as the main source of H2S. The behavior of the observed H2S abundance suggests a changing desorption efficiency, which would probe the snowline in these cold cores. Our model, however, highly overestimates the observed gas-phase CS abundance. Given the uncertainty in the sulphur chemistry, we can only conclude that our data are consistent with a cosmic elemental S abundance with an uncertainty of a factor of 10.
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Affiliation(s)
- D Navarro-Almaida
- Observatorio Astronómico Nacional (OAN), Alfonso XII, 3, 28014, Madrid, Spain
| | - R Le Gal
- Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138, USA
| | - A Fuente
- Observatorio Astronómico Nacional (OAN), Alfonso XII, 3, 28014, Madrid, Spain
| | | | - V Wakelam
- Laboratoire d'Astrophysique de Bordeaux, Univ. Bordeaux, CNRS, B18N, allée Geoffroy Saint-Hilaire, 33615 Pessac, France
| | - S Cazaux
- Faculty of Aerospace Engineering, Delft University of Technology, Delft, The Netherlands; University of Leiden, P.O. Box 9513, NL, 2300 RA, Leiden, The Netherlands
| | - P Caselli
- Centre for Astrochemical Studies, Max-Planck-Institute for Extraterrestrial Physics, Giessenbachstrasse 1, 85748, Garching, Germany
| | - Jacob C Laas
- Centre for Astrochemical Studies, Max-Planck-Institute for Extraterrestrial Physics, Giessenbachstrasse 1, 85748, Garching, Germany
| | - T Alonso-Albi
- Observatorio Astronómico Nacional (OAN), Alfonso XII, 3, 28014, Madrid, Spain
| | - J C Loison
- Institut des Sciences Moléculaires (ISM), CNRS, Univ. Bordeaux, 351 cours de la Libération, F-33400, Talence, France
| | - M Gerin
- Observatoire de Paris, PSL Research University, CNRS, École Normale Supérieure, Sorbonne Universités, UPMC Univ. Paris 06, 75005, Paris, France
| | - C Kramer
- Instituto Radioastronomía Milimétrica (IRAM), Av. Divina Pastora 7, Nucleo Central, 18012, Granada, Spain
| | - E Roueff
- Sorbonne Université, Observatoire de Paris, Université PSL, CNRS, LERMA, F-92190, Meudon, France
| | - R Bachiller
- Observatorio Astronómico Nacional (OAN), Alfonso XII, 3, 28014, Madrid, Spain
| | - B Commerçon
- École Normale Supérieure de Lyon, CRAL, UMR CNRS 5574, Université Lyon I, 46 Allée d'Italie, 69364, Lyon Cedex 07, France
| | - R Friesen
- National Radio Astronomy Observatory, 520 Edgemont Rd., Charlottesville VA USA 22901
| | - S García-Burillo
- Observatorio Astronómico Nacional (OAN), Alfonso XII, 3, 28014, Madrid, Spain
| | - J R Goicoechea
- Instituto de Física Fundamental (CSIC), Calle Serrano 123, 28006, Madrid, Spain
| | - B M Giuliano
- Centre for Astrochemical Studies, Max-Planck-Institute for Extraterrestrial Physics, Giessenbachstrasse 1, 85748, Garching, Germany
| | - I Jiménez-Serra
- Centro de Astrobiología (CSIC-INTA), Ctra. de Ajalvir, km 4, Torrejón de Ardoz, 28850, Madrid, Spain
| | - J M Kirk
- Jeremiah Horrocks Institute, University of Central Lancashire, Preston PR1 2HE, UK
| | - V Lattanzi
- Centre for Astrochemical Studies, Max-Planck-Institute for Extraterrestrial Physics, Giessenbachstrasse 1, 85748, Garching, Germany
| | - J Malinen
- Department of Physics, University of Helsinki, PO Box 64, 00014, Helsinki, Finland
- Institute of Physics I, University of Cologne, Cologne, Germany
| | - N Marcelino
- Instituto de Física Fundamental (CSIC), Calle Serrano 123, 28006, Madrid, Spain
| | - R Martín-Domènech
- Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138, USA
| | - G M Muñoz Caro
- Centro de Astrobiología (CSIC-INTA), Ctra. de Ajalvir, km 4, Torrejón de Ardoz, 28850, Madrid, Spain
| | - J Pineda
- Centre for Astrochemical Studies, Max-Planck-Institute for Extraterrestrial Physics, Giessenbachstrasse 1, 85748, Garching, Germany
| | - B Tercero
- Observatorio Astronómico Nacional (OAN), Alfonso XII, 3, 28014, Madrid, Spain
| | - S P Treviño-Morales
- Chalmers University of Technology, Department of Space, Earth and Environment, SE-412 93 Gothenburg, Sweden
| | - O Roncero
- Instituto de Física Fundamental (CSIC), Calle Serrano 123, 28006, Madrid, Spain
| | - A Hacar
- Leiden Observatory, Leiden University, PO Box 9513, 2300-RA, Leiden, The Netherlands
| | - M Tafalla
- Observatorio Astronómico Nacional (OAN), Alfonso XII, 3, 28014, Madrid, Spain
| | - D Ward-Thompson
- Jeremiah Horrocks Institute, University of Central Lancashire, Preston PR1 2HE, UK
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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. Astron Astrophys 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] [What about the content of this article? (0)] [Affiliation(s)] [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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Fuente A, Navarro DG, Caselli P, Gerin M, Kramer C, Roueff E, Alonso-Albi T, Bachiller R, Cazaux S, Commercon B, Friesen R, García-Burillo S, Giuliano BM, Goicoechea JR, Gratier P, Hacar A, Jiménez-Serra I, Kirk J, Lattanzi V, Loison JC, Malinen J, Marcelino N, Martín-Doménech R, Muñoz-Caro G, Pineda J, Tafalla M, Tercero B, Ward-Thompson D, Treviño-Morales SP, Riviére-Marichalar P, Roncero O, Vidal T, Ballester MY. Gas phase Elemental abundances in Molecular cloudS (GEMS): I. The prototypical dark cloud TMC 1. Astron Astrophys 2019; 624:10.1051/0004-6361/201834654. [PMID: 31156252 PMCID: PMC6542666 DOI: 10.1051/0004-6361/201834654] [Citation(s) in RCA: 8] [Impact Index Per Article: 1.6] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/31/2023]
Abstract
GEMS is an IRAM 30m Large Program whose aim is determining the elemental depletions and the ionization fraction in a set of prototypical star-forming regions. This paper presents the first results from the prototypical dark cloud TMC 1. Extensive millimeter observations have been carried out with the IRAM 30m telescope (3 mm and 2 mm) and the 40m Yebes telescope (1.3 cm and 7 mm) to determine the fractional abundances of CO, HCO+, HCN, CS, SO, HCS+, and N2H+ in three cuts which intersect the dense filament at the well-known positions TMC 1-CP, TMC 1-NH3, and TMC 1-C, covering a visual extinction range from A V ~ 3 to ~20 mag. Two phases with differentiated chemistry can be distinguished: i) the translucent envelope with molecular hydrogen densities of 1-5×103 cm-3; and ii) the dense phase, located at A V > 10 mag, with molecular hydrogen densities >104 cm-3. Observations and modeling show that the gas phase abundances of C and O progressively decrease along the C+/C/CO transition zone (A V ~ 3 mag) where C/H ~ 8×10-5 and C/O~0.8-1, until the beginning of the dense phase at A V ~ 10 mag. This is consistent with the grain temperatures being below the CO evaporation temperature in this region. In the case of sulfur, a strong depletion should occur before the translucent phase where we estimate a S/H ~ (0.4 - 2.2) ×10-6, an abundance ~7-40 times lower than the solar value. A second strong depletion must be present during the formation of the thick icy mantles to achieve the values of S/H measured in the dense cold cores (S/H ~8×10-8). Based on our chemical modeling, we constrain the value of ζ H2 to ~ (0.5 - 1.8) ×10-16 s-1 in the translucent cloud.
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Affiliation(s)
- A Fuente
- Observatorio Astronómico Nacional (OAN), Alfonso XII, 3, 28014, Madrid, Spain
| | - D G Navarro
- Observatorio Astronómico Nacional (OAN), Alfonso XII, 3, 28014, Madrid, Spain
| | - P Caselli
- Centre for Astrochemical Studies, Max-Planck-Institute for Extraterrestrial Physics, Giessenbachstrasse 1, 85748, Garching, Germany
| | - M Gerin
- Observatoire de Paris, PSL Research University, CNRS, École Normale Supérieure, Sorbonne Universités, UPMC Univ. Paris 06, 75005, Paris, France
| | - C Kramer
- Instituto Radioastronomía Milimétrica (IRAM), Av. Divina Pastora 7, Nucleo Central, 18012, Granada, Spain
| | - E Roueff
- Sorbonne Université, Observatoire de Paris, Université PSL, CNRS, LERMA, F-92190, Meudon, France
| | - T Alonso-Albi
- Observatorio Astronómico Nacional (OAN), Alfonso XII, 3, 28014, Madrid, Spain
| | - R Bachiller
- Observatorio Astronómico Nacional (OAN), Alfonso XII, 3, 28014, Madrid, Spain
| | - S Cazaux
- Faculty of Aerospace Engineering, Delft University of Technology, Delft, The Netherlands ; University of Leiden, P.O. Box 9513, NL, 2300 RA, Leiden, The Netherlands
| | - B Commercon
- École Normale Supérieure de Lyon, CRAL, UMR CNRS 5574, Université Lyon I, 46 Allée d'Italie, 69364, Lyon Cedex 07, France
| | - R Friesen
- National Radio Astronomy Observatory, 520 Edgemont Rd., Charlottesville VA USA 22901
| | - S García-Burillo
- Observatorio Astronómico Nacional (OAN), Alfonso XII, 3, 28014, Madrid, Spain
| | - B M Giuliano
- Centre for Astrochemical Studies, Max-Planck-Institute for Extraterrestrial Physics, Giessenbachstrasse 1, 85748, Garching, Germany
| | - J R Goicoechea
- Instituto de Física Fundamental (CSIC), Calle Serrano 123, 28006, Madrid, Spain
| | - P Gratier
- Laboratoire d'astrophysique de Bordeaux, Univ. Bordeaux, CNRS, B18N, allée Geoffroy Saint-Hilaire, 33615, Pessac, France
| | - A Hacar
- Leiden Observatory, Leiden University, PO Box 9513, 2300-RA, Leiden, The Netherlands
| | - I Jiménez-Serra
- Centro de Astrobiología (CSIC-INTA), Ctra. de Ajalvir, km 4, Torrejón de Ardoz, 28850, Madrid, Spain
| | - J Kirk
- Department of Physics, University of Warwick, Coventry CV4 7AL, UK
| | - V Lattanzi
- Centre for Astrochemical Studies, Max-Planck-Institute for Extraterrestrial Physics, Giessenbachstrasse 1, 85748, Garching, Germany
| | - J C Loison
- Institut des Sciences Moléculaires (ISM), CNRS, Univ. Bordeaux, 351 cours de la Libération, F-33400, Talence, France
| | - J Malinen
- Department of Physics, University of Helsinki, PO Box 64, 00014, Helsinki, Finland
- Institute of Physics I, University of Cologne, Cologne, Germany
| | - N Marcelino
- Instituto de Física Fundamental (CSIC), Calle Serrano 123, 28006, Madrid, Spain
| | - R Martín-Doménech
- Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA
| | - G Muñoz-Caro
- Centro de Astrobiología (CSIC-INTA), Ctra. de Ajalvir, km 4, Torrejón de Ardoz, 28850, Madrid, Spain
| | - J Pineda
- Centre for Astrochemical Studies, Max-Planck-Institute for Extraterrestrial Physics, Giessenbachstrasse 1, 85748, Garching, Germany
| | - M Tafalla
- Observatorio Astronómico Nacional (OAN), Alfonso XII, 3, 28014, Madrid, Spain
| | - B Tercero
- Observatorio Astronómico Nacional (OAN), Alfonso XII, 3, 28014, Madrid, Spain
| | - D Ward-Thompson
- Jeremiah Horrocks Institute, University of Central Lancashire, Preston PR1 2HE, UK
| | - S P Treviño-Morales
- Chalmers University of Technology, Department of Space, Earth and Environment, SE-412 93 Gothenburg, Sweden
| | | | - O Roncero
- Instituto de Física Fundamental (CSIC), Calle Serrano 123, 28006, Madrid, Spain
| | - T Vidal
- Laboratoire d'astrophysique de Bordeaux, Univ. Bordeaux, CNRS, B18N, allée Geoffroy Saint-Hilaire, 33615, Pessac, France
| | - Maikel Y Ballester
- Departamento de Física, Universidade Federal de Juiz de Fora-UFJF, Juiz de Fora, MG 36036-330, Brazil
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König S, Martín S, Muller S, Cernicharo J, Sakamoto K, Zschaechner LK, Humphreys EML, Mroczkowski T, Krips M, Galametz M, Aalto S, Vlemmings WHT, Ott J, Meier DS, Fuente A, García-Burillo S, Neri R. Sub-arcsecond imaging of the water emission in Arp 220. Astron Astrophys 2017; 602:A42. [PMID: 29151605 PMCID: PMC5687566 DOI: 10.1051/0004-6361/201630331] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/07/2023]
Abstract
AIMS Extragalactic observations of water emission can provide valuable insights into the excitation of the interstellar medium. In particular they allow us to investigate the excitation mechanisms in obscured nuclei, i.e. whether an active galactic nucleus or a starburst dominate. METHODS We use sub-arcsecond resolution observations to tackle the nature of the water emission in Arp 220. ALMA Band 5 science verification observations of the 183 GHz H2O 313-220 line, in conjunction with new ALMA Band 7 H2O 515-422 data at 325 GHz, and supplementary 22 GHz H2O 616 - 523 VLA observations, are used to better constrain the parameter space in the excitation modelling of the water lines. RESULTS We detect 183 GHz H2O and 325 GHz water emission towards the two compact nuclei at the center of Arp 220, being brighter in Arp 220 West. The emission at these two frequencies is compared to previous single-dish data and does not show evidence of variability. The 183 and 325 GHz lines show similar spectra and kinematics, but the 22 GHz profile is significantly different in both nuclei due to a blend with an NH3 absorption line. CONCLUSIONS Our findings suggest that the most likely scenario to cause the observed water emission in Arp 220 is a large number of independent masers originating from numerous star-forming regions.
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Affiliation(s)
- S König
- Chalmers University of Technology, Department of Earth and Space Sciences, Onsala Space Observatory, 43992 Onsala, Sweden
| | - S Martín
- European Southern Observatory (ESO), Alonso de Córdova 3107, Vitacura, Casilla 19001, 763 0355, Santiago, Chile
- Joint ALMA Observatory, Alonso de Córdova 3107, Vitacura, Casilla 19001, 763 0355, Santiago, Chile
| | - S Muller
- Chalmers University of Technology, Department of Earth and Space Sciences, Onsala Space Observatory, 43992 Onsala, Sweden
| | - J Cernicharo
- Grupo de Astrofísica Molecular, Instituto de CC. de Materiales de Madrid (ICMM-CSIC), Sor Juana Inés de la Cruz 3, Cantoblanco, 28049, Madrid, Spain
| | - K Sakamoto
- Institute of Astronomy and Astrophysics, Academia Sinica, PO Box 23-141, 10617, Taipei, Taiwan
| | - L K Zschaechner
- Max Planck Institute for Astronomy, Königstuhl 17, 69117 Heidelberg, Germany
| | - E M L Humphreys
- European Southern Observatory (ESO), Karl-Schwarzschild-Str. 2, 85748, Garching bei München, Germany
| | - T Mroczkowski
- European Southern Observatory (ESO), Karl-Schwarzschild-Str. 2, 85748, Garching bei München, Germany
| | - M Krips
- Institut de Radioastronomie Millimétrique (IRAM), 300 rue de la Piscine, Domaine Universitaire, 38406, Saint Martin d'Hères, France
| | - M Galametz
- Laboratoire AIM, CEA/IRFU/Service d'Astrophysique, Bât. 709, 91191, Gif-sur-Yvette, France
- European Southern Observatory (ESO), Karl-Schwarzschild-Str. 2, 85748, Garching bei München, Germany
| | - S Aalto
- Chalmers University of Technology, Department of Earth and Space Sciences, Onsala Space Observatory, 43992 Onsala, Sweden
| | - W H T Vlemmings
- Chalmers University of Technology, Department of Earth and Space Sciences, Onsala Space Observatory, 43992 Onsala, Sweden
| | - J Ott
- National Radio Astronomy Observatory (NRAO), P.O. Box O, 1003 Lopezville Road, Socorro, NM 87801, USA
| | - D S Meier
- New Mexico Institute of Mining and Technology, Socorro, NM, USA
| | - A Fuente
- Observatorio Astronómico Nacional (OAN, IGN), Apdo 112, 28803, Alcalá de Henares, Spain
| | - S García-Burillo
- Observatorio de Madrid, OAN-IGN, Alfonso XII, 3, 28014, Madrid, Spain
| | - R Neri
- Institut de Radioastronomie Millimétrique (IRAM), 300 rue de la Piscine, Domaine Universitaire, 38406, Saint Martin d'Hères, France
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Treviño-Morales SP, Fuente A, Sánchez-Monge Á, Pilleri P, Goicoechea JR, Ossenkopf-Okada V, Roueff E, Rizzo JR, Gerin M, Berné O, Cernicharo J, Gónzalez-García M, Kramer C, García-Burillo S, Pety J. The first CO + image: I. Probing the HI/H 2 layer around the ultracompact HII region Mon R2. Astron Astrophys 2016; 593:L12. [PMID: 27721515 PMCID: PMC5055094 DOI: 10.1051/0004-6361/201628899] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/06/2023]
Abstract
The CO+ reactive ion is thought to be a tracer of the boundary between a HII region and the hot molecular gas. In this study, we present the spatial distribution of the CO+ rotational emission toward the Mon R2 star-forming region. The CO+ emission presents a clumpy ring-like morphology, arising from a narrow dense layer around the HII region. We compare the CO+ distribution with other species present in photon-dominated regions (PDR), such as [CII] 158 µm, H2 S(3) rotational line at 9.3 µm, polycyclic aromatic hydrocarbons (PAHs) and HCO+. We find that the CO+ emission is spatially coincident with the PAHs and [CII] emission. This confirms that the CO+ emission arises from a narrow dense layer of the HI/H2 interface. We have determined the CO+ fractional abundance, relative to C+ toward three positions. The abundances range from 0.1 to 1.9 ×10-10 and are in good agreement with previous chemical model, which predicts that the production of CO+ in PDRs only occurs in dense regions with high UV fields. The CO+ linewidth is larger than those found in molecular gas tracers, and their central velocity are blue-shifted with respect to the molecular gas velocity. We interpret this as a hint that the CO+ is probing photo-evaporating clump surfaces.
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Affiliation(s)
- S P Treviño-Morales
- Instituto de Ciencia de Materiales de Madrid, Sor Juana Inés de la Cruz 3, E-28049 Cantoblanco, Madrid, (Spain); Observatorio Astronómico Nacional, Apdo. 112, E-28803 Alcalá de Henares Madrid, (Spain)
| | - A Fuente
- Observatorio Astronómico Nacional, Apdo. 112, E-28803 Alcalá de Henares Madrid, (Spain)
| | - Á Sánchez-Monge
- I. Physikalisches Institut, Universität zu Köln, Zülpicher Str. 77, 50937 Köln, (Germany)
| | - P Pilleri
- CNRS; IRAP; 9 Av. colonel Roche, BP 44346, F-31028 Toulouse cedex 4, (France); LERMA, Observatoire de Paris, PSL Research University, CNRS, UMR8112, Place Janssen, 92190 Meudon Cedex, (France)
| | - J R Goicoechea
- Instituto de Ciencia de Materiales de Madrid, Sor Juana Inés de la Cruz 3, E-28049 Cantoblanco, Madrid, (Spain)
| | - V Ossenkopf-Okada
- I. Physikalisches Institut, Universität zu Köln, Zülpicher Str. 77, 50937 Köln, (Germany)
| | - E Roueff
- LERMA, Observatoire de Paris, PSL Research University, CNRS, UMR8112, Place Janssen, 92190 Meudon Cedex, (France)
| | - J R Rizzo
- Centro de Astrobiología, E-28850 Torrejón de Ardoz, (Spain)
| | - M Gerin
- LERMA, Observatoire de Paris, PSL Research University, CNRS, UMR8112, Place Janssen, 92190 Meudon Cedex, (France)
| | - O Berné
- CNRS; IRAP; 9 Av. colonel Roche, BP 44346, F-31028 Toulouse cedex 4, (France); Université de Toulouse, UPS-OMP, IRAP, 31000 Toulouse, (France)
| | - J Cernicharo
- Instituto de Ciencia de Materiales de Madrid, Sor Juana Inés de la Cruz 3, E-28049 Cantoblanco, Madrid, (Spain)
| | - M Gónzalez-García
- Instituto de Astrofísica de Andalucía, CSIC, E-18008, Granada, (Spain)
| | - C Kramer
- Instituto de Radioastronomía Milimétrica, Ave. Divina Pastora, 7, Local 20 18012, Granada (Spain)
| | - S García-Burillo
- Observatorio Astronómico Nacional, Apdo. 112, E-28803 Alcalá de Henares Madrid, (Spain)
| | - J Pety
- Institut de Radioastronomie Millimétrique, 300 Rue de la Piscine, F-38406 Saint Martin d'Hères, (France)
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Genzel R, Tacconi LJ, Lutz D, Saintonge A, Berta S, Magnelli B, Combes F, García-Burillo S, Neri R, Bolatto A, Contini T, Lilly S, Boissier J, Boone F, Bouché N, Bournaud F, Burkert A, Carollo M, Colina L, Cooper MC, Cox P, Feruglio C, Förster Schreiber NM, Freundlich J, Gracia-Carpio J, Juneau S, Kovac K, Lippa M, Naab T, Salome P, Renzini A, Sternberg A, Walter F, Weiner B, Weiss A, Wuyts S. COMBINED CO AND DUST SCALING RELATIONS OF DEPLETION TIME AND MOLECULAR GAS FRACTIONS WITH COSMIC TIME, SPECIFIC STAR-FORMATION RATE, AND STELLAR MASS. ACTA ACUST UNITED AC 2015. [DOI: 10.1088/0004-637x/800/1/20] [Citation(s) in RCA: 418] [Impact Index Per Article: 46.4] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/12/2022]
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García-Burillo S, Fuente A, Martín-Pintado J, Usero A, Graciá-Carpio J, Planesas P. Extragalactic chemistry of molecular gas: lessons from the local universe. Faraday Discuss 2006; 133:33-42; discussion 83-102, 449-52. [PMID: 17191440 DOI: 10.1039/b601805j] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/21/2022]
Abstract
Observational constraints provided by high resolution and high sensitivity observations of external galaxies made in the millimetre and sub-millimetre range have started to put on a firm footing the study of the extragalactic chemistry of molecular gas. In particular, the availability of multi-species and multi-line surveys of nearby galaxies is central to the interpretation of existent and forthcoming millimetre observations of the high redshift universe. Probing the physical and chemical status of molecular gas in starbursts and active galaxies (AGN) requires the use of specific tracers of the relevant energetic phenomena that are known to be at play in these galaxies: large-scale shocks, strong UV fields, cosmic rays and X-rays. We present below the first results of an ongoing survey, allying the IRAM 30 m telescope with the Plateau de Bure interferometer (PdBI), devoted to the study of the chemistry of molecular gas in a sample of starbursts and AGN of the local universe. These observations highlight the existence of a strong chemical differentiation in the molecular disks of starbursts and AGN.
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Affiliation(s)
- S García-Burillo
- Observatorio Astronómico Nacional-OAN, Observatorio de Madrid, Alfonso XII, 3, E-28014, Spain
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