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24 results on '"Codella, Claudio"'

1. Astrochemistry of Galactic regions: living ALMA, preparing SKA

Author: Codella, Claudio
Abstract: Astrochemistry of Galactic regions is living a golden age. More specifically, the study of the so-called interstellar Complex Organic Molecules (iCOMs, mainly O-bearing species with at least 6 atoms), considered the simplest bricks needed to have pre-biotic environments, has benefited of recent improvements of observational tools. On the one hand, single-dish spectral surveys withtelescopes observing at cm-wavelengths (mainly GBT, and Yebes), once equipped with improvedbackends, increased the number of complex species detected in the interstellar medium (ISM). Onthe other hand, the advent of the ALMA (sub-)mm interferometer, with its unique combination of high sensitivity, high angular resolution, and large spectral coverage, boosted both the detections ofiCOMs and the imaging of their spatial distributions. iCOMs are almost ubiquitous in the ISM,being observed in a wide variety of astronomical environments and physical conditions: in bothcold molecular clouds and hot regions, in the Galactic disk as well as in the Galactic Center. In this context, we will review the power of ALMA in shedding light on the chemistry atwork during the earliest phases of low-mass star formation. The role of the pre-solar chemistry inthe composition of the Solar System bodies is far to be understood. Key questions still to beaddressed are: how chemically organic complex are the volatiles delivered to the pristine planetaryatmospheres? What molecules are passed from the large-scale envelope to the disk in which planets,comets, and asteroids form? As a matter of fact, molecular complexity builds up at each step of theprocess leading to star formation, ending up in prebiotic molecules. Indeed, one of the breakthroughresults found by ALMA has been imaging iCOMs emission in protostellar and protoplanetary disks.Finally, we will also discuss the limits of ALMA observations, paradoxically due to the high spatialresolution reached: the iCOMs detection is hampered by the high-opacity continuum in the diskmidplane, i.e. the region where planets are expected to form. This is a limit of the ALMA datasetsthat further sub-mm observations will never overcome. Only high spatial resolution (< 10 au)observations at much lower frequencies, at cm-wavelengths, where the dust continuum is morelikely to be optically thin, will be able to provide the answer, paving the way to the arrival of SKA.
Published: 2023
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2. Streamers feeding the SVS13-A protobinary system: astrochemistry reveals accretion shocks?'

Author: Bianchi, Eleonora, López-Sepulcre, Ana, Ceccarelli, Cecilia, Codella, Claudio, Podio, Linda, Bouvier, Mathilde, Enrique-Romero, Joan, Bachiller, Rafael, and Leflochb, Bertrand
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Physical and Theoretical Chemistry, Astrophysics - Astrophysics of Galaxies, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: We report ALMA high-angular resolution (~ 50 au) observations of the binary system SVS13-A. More specifically, we analyse deuterated water (HDO) and sulfur dioxide (SO2) emission. The molecular emission is associated with both the components of the binary system, VLA4A and VLA4B. The spatial distribution is compared to that of formamide (NH2CHO), previously analysed in the system. Deuterated water reveals an additional emitting component spatially coincident with the dust accretion streamer, at a distance larger than 120 au from the protostars, and at blue-shifted velocities (> 3 km/s from the systemic velocities). We investigate the origin of the molecular emission in the streamer, in light of thermal sublimation temperatures calculated using updated binding energies (BE) distributions. We propose that the observed emission is produced by an accretion shock at the interface between the accretion streamer and the disk of VLA4A. Thermal desorption is not completely excluded in case the source is actively experiencing an accretion burst., Accepted for publication in Faraday Discussions 2023
Published: 2023
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3. CH$_3$CN deuteration in the SVS13-A Class I hot-corino. SOLIS XV

Author: Bianchi, Eleonora, Ceccarelli, Cecilia, Codella, Claudio, López-Sepulcre, Ana, Yamamoto, Satoshi, Balucani, Nadia, Caselli, Paola, Podio, Linda, Neri, Roberto, Bachiller, Rafael, Favre, Cécile, Fontani, Francesco, Lefloch, Bertrand, Sakai, Nami, and Segura-Cox, Dominique
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics - Astrophysics of Galaxies, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: We studied the line emission from CH3CN and its deuterated isotopologue CH$_2$DCN towards the prototypical Class I object SVS13-A, where the deuteration of a large number of species has already been reported. Our goal is to measure the CH$_3$CN deuteration in a Class I protostar, for the first time, in order to constrain the CH$_3$CN formation pathways and the chemical evolution from the early prestellar core and Class 0 to the evolved Class I stages. We imaged CH2DCN towards SVS13-A using the IRAM NOEMA interferometer at 3mm in the context of the Large Program SOLIS (with a spatial resolution of 1.8"x1.2"). The NOEMA images have been complemented by the CH$_3$CN and CH$_2$DCN spectra collected by the IRAM-30m Large Program ASAI, that provided an unbiased spectral survey at 3mm, 2mm, and 1.3mm. The observed line emission has been analysed using LTE and non-LTE LVG approaches. The NOEMA/SOLIS images of CH2DCN show that this species emits in an unresolved area centered towards the SVS13-A continuum emission peak, suggesting that methyl cyanide and its isotopologues are associated with the hot corino of SVS13-A, previously imaged via other iCOMs. In addition, we detected 41 and 11 ASAI transitions of CH$_3$CN and CH2DCN, respectively, which cover upper level energies (Eup) from 13 to 442 K and from 18 K to 200 K, respectively. The derived [CH2DCN]/[CH3CN] ratio is $\sim$9\%. This value is consistent with those measured towards prestellar cores and a factor 2-3 higher than those measured in Class 0 protostars. Contrarily to what expected for other molecular species, the CH3CN deuteration does not show a decrease in SVS13-A with respect to measurements in younger prestellar cores and Class 0 protostars. Finally, we discuss why our new results suggest that CH3CN was likely synthesised via gas-phase reactions and frozen onto the dust grain mantles during the cold prestellar phase., 20 pages, 2 tables, 12 figures
Published: 2022

4. FAUST III. Misaligned rotations of the envelope, outflow, and disks in the multiple protostellar system of VLA 1623$-$2417

Author: Ohashi, Satoshi, Codella, Claudio, Sakai, Nami, Chandler, Claire J., Ceccarelli, Cecilia, Alves, Felipe, Fedele, Davide, Hanawa, Tomoyuki, Dur��n, Aurora, Favre, C��cile, L��pez-Sepulcre, Ana, Loinard, Laurent, Mercimek, Seyma, Murillo, Nadia M., Podio, Linda, Zhang, Yichen, Aikawa, Yuri, Balucani, Nadia, Bianchi, Eleonora, Bouvier, Mathilde, Busquet, Gemma, Caselli, Paola, Caux, Emmanuel, Charnley, Steven, Choudhury, Spandan, Cuello, Nicolas, De Simone, Marta, Dulieu, Francois, Evans, Lucy, Feng, Siyi, Fontani, Francesco, Francis, Logan, Hama, Tetsuya, Herbst, Eric, Hirano, Shingo, Hirota, Tomoya, Imai, Muneaki, Isella, Andrea, J��menez-Serra, Izaskun, Johnstone, Doug, Kahane, Claudine, Gal, Romane Le, Lefloch, Bertrand, Maud, Luke T., Maureira, Maria Jose, Menard, Francois, Miotello, Anna, Moellenbrock, George, Mori, Shoji, Nakatani, Riouhei, Nomura, Hideko, Oba, Yasuhiro, O'Donoghue, Ross, Okoda, Yuki, Ospina-Zamudio, Juan, Oya, Yoko, Pineda, Jaime, Rimola, Albert, Sakai, Takeshi, Segura-Cox, Dominique, Shirley, Yancy, Svoboda, Brian, Taquet, Vianney, Testi, Leonardo, Vastel, Charlotte, Viti, Serena, Watanabe, Naoki, Watanabe, Yoshimasa, Witzel, Arezu, Xue, Ci, Zhao, Bo, and Yamamoto, Satoshi
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics
Abstract: We report a study of the low-mass Class-0 multiple system VLA 1623AB in the Ophiuchus star-forming region, using H$^{13}$CO$^+$ ($J=3-2$), CS ($J=5-4$), and CCH ($N=3-2$) lines as part of the ALMA Large Program FAUST. The analysis of the velocity fields revealed the rotation motion in the envelope and the velocity gradients in the outflows (about 2000 au down to 50 au). We further investigated the rotation of the circum-binary VLA 1623A disk as well as the VLA 1623B disk. We found that the minor axis of the circum-binary disk of VLA 1623A is misaligned by about 12 degrees with respect to the large-scale outflow and the rotation axis of the envelope. In contrast, the minor axis of the circum-binary disk is parallel to the large-scale magnetic field according to previous dust polarization observations, suggesting that the misalignment may be caused by the different directions of the envelope rotation and the magnetic field. If the velocity gradient of the outflow is caused by rotation, the outflow has a constant angular momentum and the launching radius is estimated to be $5-16$ au, although it cannot be ruled out that the velocity gradient is driven by entrainments of the two high-velocity outflows. Furthermore, we detected for the first time a velocity gradient associated with rotation toward the VLA 16293B disk. The velocity gradient is opposite to the one from the large-scale envelope, outflow, and circum-binary disk. The origin of its opposite gradient is also discussed., 27 pages, 21 figures, 2 Tables, Accepted for publication in ApJ
Published: 2022

5. Exploring the link between star and planet formation with Ariel

Author: Turrini, Diego, Codella, Claudio, Danielski, Camilla, et al, Helled, Ravit, University of Zurich, and Turrini, Diego
Subjects: 1912 Space and Planetary Science, 530 Physics, Space and Planetary Science, 10231 Institute for Computational Science, 3103 Astronomy and Astrophysics, Astronomy and Astrophysics
Published: 2022
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6. AMBITION - comet nucleus cryogenic sample return

Author: Bockelée-Morvan, Dominique, Filacchione, Gianrico, Altwegg, Kathrin, Bianchi, Eleonora, Bizzarro, Martin, Blum, Jürgen, Bonal, Lydie, Capaccioni, Fabrizio, Choukroun, Mathieu, Codella, Claudio, Cottin, Hervé, Davidsson, Björn, De Sanctis, Maria C., Drozdovskaya, Maria N., Engrand, Cécile, Galand, Marina, Güttler, Carsten, Henri, Pierre, Herique, Alain, Ivanovski, Stavro, and Schönbächler, Maria
Subjects: Comets, Space missions, Solar system
Abstract: We describe the AMBITION project, a mission to return the first-ever cryogenically-stored sample of a cometary nucleus, that has been proposed for the ESA Science Programme Voyage 2050. Comets are the leftover building blocks of giant planet cores and other planetary bodies, and fingerprints of Solar System's formation processes. We summarise some of the most important questions still open in cometary science and Solar System formation after the successful Rosetta mission. We show that many of these scientific questions require sample analysis using techniques that are only possible in laboratories on Earth. We summarize measurements, instrumentation and mission scenarios that can address these questions. We emphasize the need for returning a sample collected at depth or, still more challenging, at cryogenic temperatures while preserving the stratigraphy of the comet nucleus surface layers. We provide requirements for the next generation of landers, for cryogenic sample acquisition and storage during the return to Earth. Rendezvous missions to the main belt comets and Centaurs, expanding our knowledge by exploring new classes of comets, are also discussed. The AMBITION project is discussed in the international context of comet and asteroid space exploration., Experimental Astronomy, 54 (2-3), ISSN:0922-6435, ISSN:1572-9508
Published: 2022
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7. AMBITION, the Comet Nucleus Cryogenic Sample Return mission for ESA Voyage 2050 program

Author: Filacchione, Gianrico, Bockelée-Morvan, Dominique, Altwegg, Kathrin, Bianchi, Eleonora, Bizzarro, Martin, Blum, Jürgen, Bonal, Lydie, Capaccioni, Fabrizio, Codella, Claudio, Choukroun, Mathieu, Cottin, Hervé, Davidsson, Björn, De Sanctis, Maria Cristina, Drozdovskaya, Maria, Engrand, Cécile, Galand, Marina, Güttler, Carsten, Henri, Pierre, Hérique, Alain, Ivanovski, Stavro L., Kokotanekova, Rosita, Levasseur-Regourd, Anny Chantal, Miller, Kelly E., Rotundi, Alessandra, Schönbächler, Maria, Snodgrass, Colin, Thomas, Nicolas, Tubiana, Cécilia, Ulamec, Stefan, Vincent, Jean-Baptiste, Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Physikalisches Institut [Bern], Universität Bern [Bern] (UNIBE), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Centre for Star and Planet Formation (STARPLAN), Globe Institute, Faculty of Health and Medical Sciences, University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH)-Faculty of Health and Medical Sciences, University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH), Institut für Geophysik und Extraterrestrische Physik [Braunschweig] (IGEP), Technische Universität Braunschweig = Technical University of Braunschweig [Braunschweig], INAF - Osservatorio Astrofisico di Arcetri (OAA), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Laboratoire Interuniversitaire des Systèmes Atmosphériques (LISA (UMR_7583)), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Center for Space and Habitability (CSH), University of Bern, Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Department of Physics [Imperial College London], Imperial College London, Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), INAF - Osservatorio Astronomico di Trieste (OAT), European Southern Observatory [Garching], PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Southwest Research Institute [San Antonio] (SwRI), Department of Earth Sciences [Swiss Federal Institute of Technology - ETH Zürich] (D-ERDW), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Institute for Astronomy [Edinburgh] (IfA), University of Edinburgh, Deutsches Zentrum für Luft- und Raumfahrt [Köln] (DLR), DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Cardon, Catherine, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Universität Bern [Bern], Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU)-Faculty of Health and Medical Sciences, University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU), California Institute of Technology (CALTECH)-NASA, Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National d’Études Spatiales [Paris] (CNES), and Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)
Subjects: [SDU] Sciences of the Universe [physics], [SDU]Sciences of the Universe [physics], ComputingMilieux_MISCELLANEOUS
Abstract: International audience
Published: 2020

8. Seeds of Life in Space (SOLIS)

Author: Taquet, Vianney, Codella, Claudio, De Simone, Marta, Lopez-Sepulcre, Ana, Pineda, Jaime E., Universiteit Leiden [Leiden], INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), and Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)
Subjects: [SDU]Sciences of the Universe [physics]
Abstract: International audience; Context. Low-mass protostars drive powerful molecular outflows that can be observed with millimetre and submillimetre telescopes. Various sulfuretted species are known to be bright in shocks and could be used to infer the physical and chemical conditions throughout the observed outflows. Aims. The evolution of sulfur chemistry is studied along the outflows driven by the NGC 1333-IRAS4A protobinary system located in the Perseus cloud to constrain the physical and chemical processes at work in shocks. Methods. We observed various transitions from OCS, CS, SO, and SO 2 towards NGC 1333-IRAS4A in the 1.3, 2, and 3 mm bands using the IRAM NOrthern Extended Millimeter Array and we interpreted the observations through the use of the Paris-Durham shock model. Results. The targeted species clearly show different spatial emission along the two outflows driven by IRAS4A. OCS is brighter on small and large scales along the south outflow driven by IRAS4A1, whereas SO 2 is detected rather along the outflow driven by IRAS4A2 that is extended along the north east-south west direction. SO is detected at extremely high radial velocity up to +25 km s −1 relative to the source velocity, clearly allowing us to distinguish the two outflows on small scales. Column density ratio maps estimated from a rotational diagram analysis allowed us to confirm a clear gradient of the OCS/SO 2 column density ratio between the IRAS4A1 and IRAS4A2 outflows. Analysis assuming non Local Thermodynamic Equilibrium of four SO 2 transitions towards several SiO emission peaks suggests that the observed gas should be associated with densities higher than 10 5 cm −3 and relatively warm (T > 100 K) temperatures in most cases. Conclusions. The observed chemical differentiation between the two outflows of the IRAS4A system could be explained by a different chemical history. The outflow driven by IRAS4A1 is likely younger and more enriched in species initially formed in interstellar ices, such as OCS, and recently sputtered into the shock gas. In contrast, the longer and likely older outflow triggered by IRAS4A2 is more enriched in species that have a gas phase origin, such as SO 2 .
Published: 2020
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9. AMBITION Comet Nucleus Cryogenic Sample Return

Author: Bockelée-Morvan, D., Filacchione, Gianrico, Altwegg, Kathrin, Bianchi, Eleonora, Bizzarro, Martin, Blum, Jürgen, Bonal, Lydie, Capaccioni, Fabrizio, Codella, Claudio, Choukroun, Mathieu, Cottin, Hervé, Davidsson, Björn, De Sanctis, Maria Cristina, Drozdovskaya, Maria, Engrand, Cécile, Galand, Marina, Güttler, Carsten, Henri, Pierre, Herique, Alain, Ivanoski, Stavro, Kokotanekova, Rosita, Levasseur-Regourd, Anny Chantal, Miller, Kelly E., Rotundi, Alessandra, Schönbächler, Maria, Snodgrass, Colin, Thomas, Nicolas, Tubiana, Cecilia, Ulamec, Stefan, Vincent, Jean-Baptiste, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Physikalisches Institut [Bern], Universität Bern [Bern], Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Centre for Star and Planet Formation (STARPLAN), Globe Institute, Faculty of Health and Medical Sciences, University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU)-Faculty of Health and Medical Sciences, University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU), Natural History Museum of Denmark, Faculty of Science [Copenhagen], Institut für Geophysik und Extraterrestrische Physik [Braunschweig] (IGEP), Technische Universität Braunschweig [Braunschweig], INAF - Osservatorio Astrofisico di Arcetri (OAA), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Laboratoire Interuniversitaire des Systèmes Atmosphériques (LISA (UMR_7583)), Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Center for Space and Habitability (CSH), University of Bern, Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Space and Atmospheric Physics Group [London], Blackett Laboratory, Imperial College London-Imperial College London, Department of Physics [Imperial College London], Imperial College London, Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Centre National d’Études Spatiales [Paris] (CNES), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Trieste (OAT), European Southern Observatory (ESO), IMPEC - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Southwest Research Institute [San Antonio] (SwRI), Department of Earth Sciences [ETH Zürich] (D-ERDW), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), Institute for Astronomy [Edinburgh] (IfA), University of Edinburgh, German Aerospace Center (DLR), DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Technische Universität Braunschweig = Technical University of Braunschweig [Braunschweig], Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National d’Études Spatiales [Paris] (CNES), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), PLANETO - LATMOS, Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Department of Earth Sciences [Swiss Federal Institute of Technology - ETH Zürich] (D-ERDW), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), California Institute of Technology (CALTECH)-NASA, Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12)-Institut national des sciences de l'Univers (INSU - CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, and COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), [SDU]Sciences of the Universe [physics], FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics - Earth and Planetary Astrophysics
Abstract: This white paper proposes that AMBITION, a Comet Nucleus Sample Return mission, be a cornerstone of ESA's Voyage 2050 programme. We summarise some of the most important questions still open in cometary science after the successes of the Rosetta mission, many of which require sample analysis using techniques that are only possible in laboratories on Earth. We then summarise measurements, instrumentation and mission scenarios that can address these questions, with a recommendation that ESA select an ambitious cryogenic sample return mission. Rendezvous missions to Main Belt comets and Centaurs are compelling cases for M-class missions, expanding our knowledge by exploring new classes of comets. AMBITION would engage a wide community, drawing expertise from a vast range of disciplines within planetary science and astrophysics. With AMBITION, Europe will continue its leadership in the exploration of the most primitive Solar System bodies., 8 figures, 26 pages
Published: 2019

10. The GENESIS-SKA project: looking for Solar System analogs

Author: Codella, Claudio
Abstract: The recipe to make a habitable planet like our own Earth requires a relatively small rocky planet, at the right distance from the host star, with a not-too-thick atmosphere which should be rich in volatiles and capable of developing complex organic molecules chemistry. Searches for exoplanets have shown a large degree of diversity among planetary systems, but have left still unanswered the two fundamental questions of how common planetary systems like our own are and of how general are the processes that allow for creating habitable planets. Understanding the formation of planetary systems and the chemical processing of the volatiles that are going to form their atmospheres is therefore key to understand the origins of the Solar System. Key questions still to be addressed are: (i) how solids overcome the growth barriers to become rocky cores, (ii) how the formation of giant planets and their interaction with gas and solids in disks affect the formation of planets, and (iii) how chemically complex are the volatiles delivered on the pristine planetary atmospheres. The SKA telescope, and more specifically the GENESIS-SKA project, will allow us to study in detail the evolution of dust as it evolves into planetesimals and rocky planets and to detect heavy complex organic molecules that today are beyond the reach of our observing capabilities. The GENESIS-SKA project, supported as PRIN-INAF, is carrying on studies on dust evolution, planet formation, and pre-biotic chemical complexity, in the context of preparation of SKA Key Programmes. More specifically, we are featuring a brand new synergy (in the INAF framework) between astronomical observational (e.g. VLA, GBT, ALMA, IRAM, LBT, VLT) and modeling efforts, laboratory experiments, and state-of-the-art quantum-chemical computations.
Published: 2018
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11. Young Stars and their Variability with LSST

Author: Bonito, Rosaria, Hartigan, Patrick, Venuti, Laura, Guarcello, Mario, Prisinzano, Loredana, Argiroffi, Costanza, Messina, Sergio, Johns-Krull, Christopher, Feigelson, Eric, Stauffer, John, Giannini, Teresa, Antoniucci, Simone, Sciortino, Salvo, Micela, Giusi, Pillitteri, Ignazio, Fedele, Davide, Podio, Linda, Damiani, Francesco, McGehee, Peregrine, Street, Rachel, Gizis, John, Sacco, Germano, Magrini, Laura, Flaccomio, Ettore, Orlando, Salvatore, Miceli, Marco, Stelzer, Beate, Fuchs, Julien, Chen, Sophia, Pikuz, Sergey, Frasca, Antonio, Biazzo, Katia, Codella, Claudio, Pastorello, Andrea, Alcala', Juan Manuel, Covino, Elvira, Bianchi, Eleonora, and Nisini, Brunella
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: Young stars exhibit short-term photometric variability caused by mass accretion events from circumstellar disks, the presence of dusty warps within the inner disks, starspots that rotate across the stellar surfaces, and flares. Long-term variability also occurs owing to starspot longevity and cycles, and from changes in stellar angular momenta and activity as the stars age. We propose to observe the Carina star-forming region in different bands with a cadence of 30 minutes every night for one week per year to clarify the nature of both the short-term and long-term variability of the thousands of young stars in this region. By obtaining well-sampled multicolor lightcurves of this dense young cluster, LSST would acquire the first statistically significant data on how these objects vary on both short and long timescales. This information will allow us to relate the observed variability to stellar properties such as mass, age, binarity, and to environmental properties such as location within or exterior to the H II region, and to the presence or absence of a circumstellar disk., Comment: Contribution in response of the Call for White Papers on LSST Cadence Optimization
Published: 2018
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12. The Chemistry Of Protostellar Jet-Disk Systems

Author: Codella Claudio
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: The birth of a Sun-like star is a complex game played by several participants whose respective roles are not yet entirely clear. On the one hand, the star-to-be accretes matter from a collapsing envelope. The gravitational energy released in the process heats up the material surrounding the protostar, creating warm regions enriched by interstellar complex organic molecules (iCOMs, at least 6 atoms) called hot-corinos. On the other hand, the presence of angular momentum and magnetic fields leads to two consequences: (i) the formation of circumstellar disks; and (ii) substantial episodes of matter ejection, as e.g. collimated jets. Thanks to the combination of the high-sensitivities and high-angular resolu- tions provided by the advent of new telescopes such as ALMA and NOEMA, it is now possible to image in details the earliest stages of the Sun-like star formation, thus inspecting the inner ( < 50 AU from the protostar) jet. At these spatial scales a proper study of jets has to take into account also the effects connected with the accreting disk. In other words, it is time to study the protostellar jet-disk system as a whole. Several still unanswered questions can be addressed. What is the origin of the chemically enriched hot corinos: are they jet-driven shocked regions? What is the origin of the ejections: are they due to disk or stellar winds? Shocks are precious tool to attack these questions, given they enrich the gas phase with the species deposited onto the dust mantles and/or locked in the refractory dust cores. Basically, we have to deal with two kind of shocks: (i) high-velocity shocks produced by protostellar jets, and (ii) slow accretion shocks located close to the centrifugal barrier of the accretion disks. Both shocks are factories of iCOMs, which can be then efficiently used to follow both the kinematics and the chemistry of the inner protostellar systems. With this in mind, we will discuss recent results obtained in the framework of different observational campaigns at mm and sub-mm wavelengths.&nbsp
Published: 2017
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13. H2S in the L1157-B1 Bow shock

Author: Holdship, Jonathan, Viti, Serena, Jimenez-Serra, Izaskun, Lefloch, Bertrand, Codella, Claudio, Podio, Linda, Benedettini, Milena, Fontani, Francesco, Bachiller, Rafael, Tafalla, Mario, and Ceccarelli, Cecilia
Subjects: Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences
Abstract: Sulfur-bearing molecules are highly reactive in the gas phase of the ISM. However, the form in which most of the sulfur is locked onto interstellar dust grains is unknown. By taking advantage of the short time-scales of shocks in young molecular outflows, one could track back the main form of sulfur in the ices. In this paper, six transitions of H$_2$S and its isotopologues in the L1157-B1 bowshock have been detected using data from the Herschel-CHESS survey and the IRAM-30m ASAI large program. These detections are used to calculate the properties of H$_2$S gas in L1157-B1 through use of a rotation diagram and to explore the possible carriers of sulfur on the grains. The isotopologue detections allow the first calculation of the H$_2$S deuteration fraction in an outflow from a low mass protostar. The fractional abundance of H$_2$S in the region is found to be 6.0$\times$10$^{-7}$ and the deuteration fraction is 2$\times$10$^{-2}$. In order to investigate the form of sulfur on the grains, a chemical model is run with four different networks, each with different branching ratios for the freeze out of sulfur bearing species into molecules such as OCS and H$_2$S. It is found that the model best fits the data when at least half of each sulfur bearing species hydrogenates when freezing. We therefore conclude that a significant fraction of sulfur in L1157-B1 is likely to be locked in H$_2$S on the grains., 10 Pages, 7 Figures. Accepted for publication in MNRAS
Published: 2016
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14. A proto-planetary disk revealed by the Herschel satellite

Author: Podio, Linda and Codella, Claudio
Subjects: Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: Herschel opened a new window on the study of the physical processes occurring when a star forms. Observations of the prototypical young star T Tau N revealed all the crucial ingredients known to be involved in star formation, namely: the parental cloud, the supersonic outflows driven by the forming star and the proto-planetary disk rotating around it. From the emission lines of the CN molecule we can estimate important disk properties, such as the disk size, inclination, and mass. The latter is roughly equal to the minimum mass of the solar nebula required to form the solar system, suggesting that the disk around T Tau N could form a planetary system like our own., Il Colle di Galileo, Vol 3, No 2 (2014)
Published: 2014
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15. The water trail from the cradle of a young Sun to Earth-like planets

Author: Podio, Linda and Codella, Claudio
Subjects: Arte, Arte. Generalidades
Abstract: El agua es un ingrediente crucial para la vida. Una de las áreas de investigación más fascinantes en el campo de la astrobiología y la astroquímica es la del origen del agua sobre la Tierra. Sabemos que nuestros océanos contienen una cantidad de agua igual a 3 diezmilésimas de la masa terrestre. Sin embargo, si consideramos también el agua presente bajo la costra terrestre, el total podría aumentar a entre 10 y 50 veces más. Existen muchas cuestiones por resolver, como por ejemplo: ¿Cuándo y cómo apareció el agua sobre la Tierra? ¿Nuestro planeta es un caso especial o hay agua, y posiblemente vida, en otros planetas de nuestra Galaxia? Con más de 1000 exoplanetas descubiertos y las estadísticas que indican que cada estrella alberga al menos un planeta, la búsqueda de agua en el universo es cada vez más urgente.
Published: 2014

16. From Clouds to Young Stellar Objects and back again: the all-in-one view from the Herschel infrared Galactic Plane Survey

Author: Molinari, Sergio, Abergel, Alain, Rivera-Ingraham, Alana, Noriega-Crespo, Alberto, Traficante, Alessio, Di Giorgio, Anna, Zavagno, Annie, Chrysostomou, Antonio, Roy, Arabino, Babar, Ali, Maiolo, Berlinda, Schulz, Bernhard, Jiang, Biwei, Sibthorpe, Bruce, Swinyard, Bruce, Battersby, Cara, Burigana, Carlo, Brunt, Chris, Davis, Chris, Joblin, Christine, Waelkens, Christoffel, Meny, Claude, Codella, Claudio, Popescu, Cristina, Polychroni, Danae, Eden, David, Ikhenaode, David, Elia, Davide, Paradis, Deborah, Shepherd, Debra, Russeil, Delphine, Ward-Thompson, D., Stamatellos, Dimitris, Marshall, Douglas, Sturm, Eckhard, Rosolowsky, Erik, Schisano, Eugenio, Faustini, Fabiana, Agostini, Fabio, Massi, Fabrizio, La Morgia, Federico, Piacentini, Francesco, Strafella, Francesco, Boulanger, Francois, Schuller, Frederic, Motte, Frederique, Wyrowski, Friedrich, Fuller, Gary, de Gasperis, Giancarlo, Joncas, Gilles, Giardino, Giovanna, White, Glenn, Umana, Grazia, Lagache, Guilaine, Rivest, Guillaume, Stringfellow, Guy, Yorke, Harold, Ristorcelli, Isabelle, Difrancesco, James, Brand, Jan, Glenn, Jason, Kirk, Jason, Rodon, Javier, Baluteau, Jean-Paul, Bernard, Jean-Philippe, Li, Jinzeng, Neves, Joao, Mottram, Joe, Fischera, Joerg, Bally, John, Richer, John, Blommaert, Joris, Cernicharo, Jose, Ganga, K., Morgan, Larry, Testi, Leonardo, Anderson, Loren, Piazzo, Lorenzo, Campeggio, Loretta, Conversi, Luca, Olmi, Luca, Valenziano, Luca, Montier, Ludovic, Spinoglio, Luigi, Beltran, Maite, Huang, Maohai, Miville-Deschenes, Marc-Antoine, Sauvage, Marc, Veneziani, Marcella, Thompson, Mark, Cohen, Martin, Giard, Martin, Marengo, Massimo, Compiegne, Mathieu, Griffin, Matt, Pomares, Melanie, Hoare, Melvin, Barlow, Michael, Burton, Michael, Reid, Michael, Smith, Michael, Pestalozzi, Michele, Juvela, Mika, Matsuura, Mikako, Benedettini, Milena, Schneider, N., Billot, Nicolas, Peretto, Nicolas, Berne, Olivier, Caselli, Paola, Debernardis, Paolo, Natoli, Paolo, Saraceno, Paolo, Goldsmith, Paul, Garcia Lario, Pedro, Martin, Peter, Schilke, Peter, Lucas, Phil, Andre, Philippe, Royer, Pierre, Zhang, Qizhou, Plume, Rene, Cesaroni, Riccardo, Tuffs, Richard, Paladini, Roberta, Vavrek, Roland, Taylor, Russ, Carey, Sean, Viti, Serena, Masi, Silvia, Pezzuto, Stefano, Lord, Steve, Chakrabarti, Sukanya, Bontemps, Sylvain, Lim, Tanya, Mueller, Thomas, Robitaille, Thomas, Troost, Tobias, Moore, Toby, Minier, Vincent, Reach, William, Fukui, Yasuo, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire Astronomique de Marseille Provence (OAMP), Université de Provence - Aix-Marseille 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Météo-France -Institut de Recherche pour le Développement (IRD)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Service de Neurologie [CHU Pitié-Salpêtrière], IFR70-CHU Pitié-Salpêtrière [AP-HP], Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP), Neurologie et thérapeutique expérimentale, Université Pierre et Marie Curie - Paris 6 (UPMC)-IFR70-Institut National de la Santé et de la Recherche Médicale (INSERM), INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), Laboratoire de Physique des Lasers (LPL), Université Paris 13 (UP13)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Radioastronomie (MPIFR), SLAC National Accelerator Laboratory (SLAC), Stanford University, Istituto di Radioastronomia [Bologna] (IRA), Center for Astrophysics and Space Astronomy [Boulder] (CASA), University of Colorado [Boulder], Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Centro de Investigaciones Biológicas (CSIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), APC - Cosmologie, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Antarctic Research a European Network for Astrophysics (ARENA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Department of Mechanical and Aerospace Engineering [Victoria]], Monash University [Clayton], Istituto Nazionale di Geofisica e Vulcanologia – Sezione di Pisa (INGV), Istituto Nazionale di Geofisica e Vulcanologia, Department of Physics and Astronomy, University of Canterbury [Christchurch], University of Manchester [Manchester], Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), I. Physikalisches Institut [Köln], Universität zu Köln, Recherche en épidémiologie et biostatistique, Université Paris-Sud - Paris 11 (UP11)-Institut National de la Santé et de la Recherche Médicale (INSERM), Laboratoire de Nanotechnologie et d'Instrumentation Optique (LNIO), Institut Charles Delaunay (ICD), Université de Technologie de Troyes (UTT)-Centre National de la Recherche Scientifique (CNRS)-Université de Technologie de Troyes (UTT)-Centre National de la Recherche Scientifique (CNRS), Institute of Atomic Physics, Université de Roumanie, Department of Physics and Astronomy [Calgary], University of Calgary, FORMATION STELLAIRE 2010, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB), Max-Planck-Institut für Extraterrestrische Physik (MPE), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Service de neurologie 1 [CHU Pitié-Salpétrière], Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-CHU Pitié-Salpêtrière [AP-HP], Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Sorbonne Université (SU)-Sorbonne Université (SU), Institut National de la Santé et de la Recherche Médicale (INSERM)-IFR70-Université Pierre et Marie Curie - Paris 6 (UPMC), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Sorbonne Université (SU)-Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Sorbonne Université (SU)-Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP), California Institute of Technology (CALTECH)-NASA, Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Assistance publique - Hôpitaux de Paris (AP-HP) (APHP)-CHU Pitié-Salpêtrière [APHP], Université Sorbonne Paris Cité (USPC)-Institut Galilée-Université Paris 13 (UP13)-Centre National de la Recherche Scientifique (CNRS), Stanford Linear Accelerator Center (SLAC), Stanford University [Stanford], Istituto di Radioastronomia (IRA), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Institut National de la Santé et de la Recherche Médicale (INSERM), Centre National de la Recherche Scientifique (CNRS)-Université de Technologie de Troyes (UTT)-Centre National de la Recherche Scientifique (CNRS)-Université de Technologie de Troyes (UTT), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), CHU Pitié-Salpêtrière [AP-HP], Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Sorbonne Université (SU), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Universität zu Köln = University of Cologne, Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), and Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB)
Subjects: [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astrophysics::Galaxy Astrophysics
Abstract: Symposium E, session 14, paper number E14-0026-10 (Oral); From diffuse interstellar cirrus to dense atomic and molecular clouds, from protostellar to post-AGB envelopes, from super-shells to supernovae remnants, the Herschel Hi-GAL survey offer an unprecedented snapshot of all the different phases of the Galactic ISM, its evolution and interactions. I will present early results on a variety of topics including the lifetime of massive pre-stellar phases, the fragmentation and collapse of extended structures, the timeline for massive star formation, dust properties in cirrus and molecular clouds.
Published: 2010

17. The clumpy structure of the chemically active L1157 outflow

Author: BENEDETTINI, Milena, VITI, Serena, CODELLA, Claudio, BACHILLER, Rafael, GUETH, Frederic, BELTRÀN, Maria T., DUTREY, Anne, GUILLOTEAU, S., Institut de RadioAstronomie Millimétrique (IRAM), Centre National de la Recherche Scientifique (CNRS), Departamento de Fisica Teorica, Universidad Autonoma de Madrid (UAM), Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire aquitain des sciences de l'univers (OASU), Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), ITA, GBR, and FRA
Subjects: [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract: We present high spatial resolution maps, obtained with the Plateau de Bure Interferometer, of the blue lobe of the L1157 outflow. We observed four lines at 3 mm, namely CH3OH (2_K-1_K), HC3N (11-10), HCN (1-0) and OCS (7-6). Moreover, the bright B1 clump has also been observed at better spatial resolution in CS (2-1), CH3OH (2_1-1_1)A-, and 34SO (3_2-2_1). These high spatial resolution observations show a very rich structure in all the tracers, revealing a clumpy structure of the gas superimposed to an extended emission. In fact, the three clumps detected by previous IRAM-30m single dish observations have been resolved into several sub-clumps and new clumps have been detected in the outflow. The clumps are associated with the two cavities created by two shock episodes driven by the precessing jet. In particular, the clumps nearest the protostar are located at the walls of the younger cavity with a clear arch-shape form while the farthest clumps have slightly different observational characteristics indicating that they are associated to the older shock episode. The emission of the observed species peaks in different part of the lobe: the east clumps are brighter in HC3N (11-10), HCN (1-0) and CS (2-1) while the west clumps are brighter in CH3OH(2_K-1_K), OCS (7-6) and 34SO (3_2-2_1). This peak displacement in the line emission suggests a variation of the physical conditions and/or the chemical composition along the lobe of the outflow at small scale, likely related to the shock activity and the precession of the outflow. In particular, we observe the decoupling of the silicon monoxide and methanol emission, common shock tracers, in the B1 clump located at the apex of the bow shock produced by the second shock episode., Comment: 11 pages, 8 figures, accepted for publication in the MNRAS
Published: 2007
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18. Extended map of TMC-1 in cyanodiacetylene

Author: Scappini, Flavio, Palumbo, Giorgio, Bruni, Gabriele, COMORETTO, Giovanni, and CODELLA, CLAUDIO
Published: 1991

19. The low-mass YSO CB230-A: investigating the protostar and its jet with NIR spectroscopy and Spitzer observations

Author: Wouterloot, Jan, Massi, Fabrizio, Codella, Claudio, Brand, Jan, Di Fabrizio, Luca, Wouterloot, J., Di Fabrizio, L., Brand, J., Codella, C., and Massi, F.
Subjects: Physics, Photosphere, Jet (fluid), Astrophysics::High Energy Astrophysical Phenomena, Near-infrared spectroscopy, Extinction (astronomy), Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Spectral line, Spitzer Space Telescope, Space and Planetary Science, Protostar, Astrophysics::Solar and Stellar Astrophysics, Emission spectrum, Astrophysics::Galaxy Astrophysics
Abstract: A jet from the low-mass YSO CB230-A had been discovered in NIR narrow-band images. We aim to investigate the physical properties of the region from where the jet is launched. Our analysis was carried out using low-resolution NIR spectra acquired with the camera NICS at the TNG telescope, with JH and HK grisms and a 1 arcsec-wide slit. These observational data were complemented with infrared photometric data from the Spitzer space telescope archive. The relevant physical properties of CB230-A were constrained by SED fitting of fluxes from the NIR to the mm. The YSO spectrum exhibits a significant number of atomic and molecular emission and absorption features. The characteristics of this spectrum suggest that we are observing a region in the close vicinity of CB230-A, i. e. its photosphere and/or an active accretion disk. The spectra of the knots in the jet contain a large number of emission lines, including a rich set of [FeII] lines. Emission due to H2 and [FeII] are not spatially correlated, confirming that [FeII] and H2 are excited by different mechanisms, in agreement with the models where [FeII] traces dissociative J-shocks and molecular hydrogen traces slower C-shocks. By using intensity ratios involving density-sensitive [FeII] lines, we estimated the electron densities in the jet (6x10^3-1x10^4 cm^-3). This indicates either high density post-shock regions of ionised gas or regions with a high degree of ionisation. By combining the present data with previously obtained maps at NIR- and mm-wavelengths, the emerging scenario is that CB230-A is a Class 0/I YSO driving an atomic jet that is observed to be almost monopolar probably due to its inclination to the plane of the sky and the resulting higher extinction of its red side. This jet appears energetic enough to drive the molecular outflow observed in the mm., Comment: 14 pages, 7 figures, accepted for publication in Astronomy and Astrophysics

20. From Clouds to Young Stellar Objects and back again: the all-in-one view from the Herschel infrared Galactic Plane Survey

Author: Molinari, Sergio, Abergel, Alain, Rivera-Ingraham, Alana, Noriega-Crespo, Alberto, Traficante, Alessio, Di Giorgio, Anna, Zavagno, Annie, Chrysostomou, Antonio, Roy, Arabino, Babar, Ali, Maiolo, Berlinda, Schulz, Bernhard, Jiang, Biwei, Sibthorpe, Bruce, Swinyard, Bruce, Battersby, Cara, Burigana, Carlo, Brunt, Chris, Davis, Chris, Joblin, Christine, Waelkens, Christoffel, Meny, Claude, Codella, Claudio, Popescu, Cristina, Polychroni, Danae, Eden, David, Ikhenaode, David, Elia, Davide, Paradis, Deborah, Shepherd, Debra, Russeil, Delphine, Ward-Thompson, Derek, Stamatellos, Dimitris, Marshall, Douglas, Sturm, Eckhard, Rosolowsky, Erik, Schisano, Eugenio, Faustini, Fabiana, Agostini, Fabio, Massi, Fabrizio, La Morgia, Federico, Piacentini, Francesco, Strafella, Francesco, Boulanger, Francois, Schuller, Frederic, Motte, Frederique, Wyrowski, Friedrich, Fuller, Gary, Gasperis, Giancarlo, Joncas, Gilles, Giardino, Giovanna, White, Glenn, Umana, Grazia, Lagache, Guilaine, Rivest, Guillaume, Stringfellow, Guy, Yorke, Harold, Ristorcelli, Isabelle, Difrancesco, James, Brand, Jan, Glenn, Jason, Kirk, Jason, Rodon, Javier, Baluteau, Jean-Paul, Bernard, Jean-Philippe, Li, Jinzeng, Neves, Joao, Mottram, Joe, Fischera, Joerg, Bally, John, Richer, John, Blommaert, Joris, Cernicharo, Jose, Ganga, Ken, Morgan, Larry, Testi, Leonardo, Anderson, Loren, Piazzo, Lorenzo, Campeggio, Loretta, Conversi, Luca, Olmi, Luca, Valenziano, Luca, Montier, Ludovic, Spinoglio, Luigi, Beltran, Maite, Huang, Maohai, Miville-Deschenes, Marc-Antoine, Sauvage, Marc, Veneziani, Marcella, Thompson, Mark, Cohen, Martin, Giard, Martin, Massimo Marengo, Compiegne, Mathieu, Griffin, Matt, Pomares, Melanie, Hoare, Melvin, Barlow, Michael, Burton, Michael, Reid, Michael, Smith, Michael, Pestalozzi, Michele, Juvela, Mika, Matsuura, Mikako, Benedettini, Milena, Schneider, Nicola, Billot, Nicolas, Peretto, Nicolas, Berne, Olivier, Caselli, Paola, Debernardis, Paolo, Natoli, Paolo, Saraceno, Paolo, Goldsmith, Paul, Garcia Lario, Pedro, Martin, Peter, Schilke, Peter, Lucas, Phil, Andre, Philippe, Royer, Pierre, Zhang, Qizhou, Plume, Rene, Cesaroni, Riccardo, Tuffs, Richard, Paladini, Roberta, Vavrek, Roland, Taylor, Russ, Carey, Sean, Viti, Serena, Masi, Silvia, Pezzuto, Stefano, Lord, Steve, Chakrabarti, Sukanya, Bontemps, Sylvain, Lim, Tanya, Mueller, Thomas, Robitaille, Thomas, Troost, Tobias, Moore, Toby, Minier, Vincent, Reach, William, and Fukui, Yasuo
Subjects: Settore FIS/05 - Astronomia e Astrofisica

21. Possible scenarios for SiS formation in the interstellar medium: Electronic structure calculations of the potential energy surfaces for the reactions of the SiH radical with atomic sulphur and S2

Author: Marzio Rosi, Nadia Balucani, Bertrand Lefloch, Dimitrios Skouteris, Noelia Faginas Lago, Cecilia Ceccarelli, Luca Mancini, Linda Podio, Claudio Codella, Rosi, Marzio, Mancini, Luca, Skouteris, Dimitrio, Ceccarelli, Cecilia, Faginas Lago, Noelia, Podio, Linda, Codella, Claudio, Lefloch, Bertrand, and Balucani, Nadia
Subjects: Physics and Astronomy (all), Physical and Theoretical Chemistry, Materials science, General Physics and Astronomy, chemistry.chemical_element, Electronic structure, 010402 general chemistry, 01 natural sciences, Potential energy, Sulfur, 0104 chemical sciences, Characterization (materials science), Interstellar medium, chemistry, Chemical physics, 0103 physical sciences, Current (fluid), 010303 astronomy & astrophysics
Abstract: In this Letter we report on the first characterization of the reactions SiH + S and SiH + S2 by means of electronic structure calculations of the stationary points along the reactive potential energy surfaces. According to our calculations, both reactions are barrierless and can lead to the formation of SiS (a species observed in interstellar objects) for which there are no convincing formation routes in current astrochemical models. Furthermore, we have verified that SiS2 cannot be considered an interstellar reservoir of sulphur because it is easily attacked by the abundant H atoms.
Published: 2018

22. Laboratory measurements and astronomical search for cyanomethanimine

Author: Rafael Bachiller, Luca Dore, Alessio Melli, Vincenzo Barone, Mattia Melosso, Cecilia Ceccarelli, Lorenzo Spada, Cristina Puzzarini, Claudio Codella, José Cernicharo, Bertrand Lefloch, C. Degli Esposti, Melosso, M., Melli, A., Puzzarini, C., Codella, C., Spada, L., Dore, L., Degli Esposti, C., Lefloch, B., Bachiller, R., Ceccarelli, C., Cernicharo, J., Barone, V., Codella, Claudio, Dipartimento di Chimica 'Giacomo Ciamician', Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Edinburgh Napier University, Dipartimento di Chimica 'G. Ciamician', Instituto Geografico Nacional (IGN), Istituto Nazionale di Astrofisica (INAF), Instituto de Ciencia de Materiales de Madrid (ICMM), and Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)
Subjects: 010504 meteorology & atmospheric sciences, Methods: laboratory: molecular, laboratory: molecular [Methods], FOS: Physical sciences, Context (language use), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, ISM: molecule, 01 natural sciences, Article, 0103 physical sciences, Astronomical interferometer, Sagittarius B2, molecule [ISM], Absorption (electromagnetic radiation), 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Physics, Spectrometer, Star formation, Molecular data, Astronomy and Astrophysics, Astronomy and Astrophysic, Astrophysics - Astrophysics of Galaxies, methods: data analysis, ISM: molecules, 3. Good health, data analysi [Methods], Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Antenna (radio), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Radio wave, Methods: data analysi
Abstract: C-cyanomethanimine (HNCHCN), existing in the two $Z$ and $E$ isomeric forms, is a key prebiotic molecule, but, so far, only the $E$ isomer has been detected toward the massive star-forming region. Sagittarius B2(N) using transitions in the radio wavelength domain. With the aim of detecting HNCHCN in Sun-like-star forming regions, the laboratory investigation of its rotational spectrum has been extended to the millimeter-/submillimeter-wave (mm-/submm-) spectral window in which several unbiased spectral surveys have been already carried out. High-resolution laboratory measurements of the rotational spectrum of C-cyanomethanimine were carried out in the 100-420 GHz range using a frequency-modulation absorption spectrometer. We then searched for the C-cyanomethanimine spectral features in the mm-wave range using the high-sensitivity and unbiased spectral surveys obtained with the IRAM 30-m antenna in the ASAI context, the earliest stages of star formation from starless to evolved Class I objects being sampled. For both the $Z$ and $E$ isomers, the spectroscopic work has led to an improved and extended knowledge of the spectroscopic parameters, thus providing accurate predictions of the rotational signatures up to $\sim$700 GHz. So far, no C-cyanomethanimine emission has been detected toward the ASAI targets, and upper limits of the column density of $\sim$ 10$^{11}$--10$^{12}$ cm$^{-2}$ could only be derived. Consequently, the C-cyanomethanimine abundances have to be less than a few 10$^{-10}$ for starless and hot-corinos. A less stringent constraint, $\leq$ 10$^{-9}$, is obtained for shocks sites. The combination of the upper limits of the abundances of C-cyanomethanimine together with accurate laboratory frequencies up to $\sim$ 700 GHz poses the basis for future higher sensitivity searches around Sun-like-star forming regions., 9 pages, 4 figures, 2 tables. A&A accepted
Published: 2018
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23. Zeeman effect in sulfur monoxide: A tool to probe magnetic fields in star forming regions

Author: Cristina Puzzarini, Jürgen Gauss, Andrés Asensio Ramos, Gabriele Cazzoli, Claudio Codella, Valerio Lattanzi, José Cernicharo, Sonia Coriani, Cazzoli, Gabriele, Lattanzi, Valerio, Coriani, Sonia, Gauss, Jürgen, Codella, Claudio, Ramos, Andrés Asensio, Cernicharo, José, Puzzarini, Cristina, European Cooperation in Science and Technology, Ministerio de Economía y Competitividad (España), Ministerio de Ciencia e Innovación (España), Università di Bologna, Ministero dell'Istruzione, dell'Università e della Ricerca, European Research Council, and German Research Foundation
Subjects: Methods: laboratory: molecular, laboratory: molecular [Methods], Context (language use), ISM: molecule, Radiation, 01 natural sciences, 7. Clean energy, Article, symbols.namesake, chemistry.chemical_compound, Methods: data analysis, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Physics::Atomic Physics, Spectral resolution, data analysis [Methods], 010303 astronomy & astrophysics, molecules [ISM], Astrophysics::Galaxy Astrophysics, Condensed Matter::Quantum Gases, Physics, Zeeman effect, Sulfur monoxide, 010304 chemical physics, Spectrometer, Star formation, Molecular data, Astronomy and Astrophysics, Astronomy and Astrophysic, ISM: molecules, Magnetic field, chemistry, Space and Planetary Science, Magnetic fields, symbols, Atomic physics, Methods: data analysi
Abstract: [Context] Magnetic fields play a fundamental role in star formation processes and the best method to evaluate their intensity is to measure the Zeeman effect of atomic and molecular lines. However, a direct measurement of the Zeeman spectral pattern from interstellar molecular species is challenging due to the high sensitivity and high spectral resolution required. So far, the Zeeman effect has been detected unambiguously in star forming regions for very few non-masing species, such as OH and CN., [Aims] We decided to investigate the suitability of sulfur monoxide (SO), which is one of the most abundant species in star forming regions, for probing the intensity of magnetic fields via the Zeeman effect., [Methods] We investigated the Zeeman effect for several rotational transitions of SO in the (sub-)mm spectral regions by using a frequency-modulated, computer-controlled spectrometer, and by applying a magnetic field parallel to the radiation propagation (i.e., perpendicular to the oscillating magnetic field of the radiation). To support the experimental determination of the g factors of SO, a systematic quantum-chemical investigation of these parameters for both SO and O has been carried out., [Results] An effective experimental-computational strategy for providing accurate g factors as well as for identifying the rotational transitions showing the strongest Zeeman effect has been presented. Revised g factors have been obtained from a large number of SO rotational transitions between 86 and 389 GHz. In particular, the rotational transitions showing the largest Zeeman shifts are: N,J = 2, 2-1, 1 (86.1 GHz), N,J = 4, 3-3, 2 (159.0 GHz), N,J = 1, 1-0, 1 (286.3 GHz), N,J = 2, 2-1, 2 (309.5 GHz), and N,J = 2, 1-1, 0 (329.4 GHz). Our investigation supports SO as a good candidate for probing magnetic fields in high-density star forming regions., This work has been supported in Bologna by MIUR “PRIN 2012, 2015” funds (project “STAR: Spectroscopic and computational Techniques for Astrophysical and atmospheric Research” – Grant Number 20129ZFHFE, project “STARS in the CAOS (Simulation Tools for Astrochemical Reactivity and Spectroscopy in the Cyberinfrastructure for Astrochemical Organic Species)” – Grant Number 2015F59J3R) and by the University of Bologna (RFO funds), in Mainz by the Deutsche Forschungsgemeinschaft (DFG 370/6-1 and 370/6-2). S.C. acknowledges support from the AIAS-COFUND program, grant agreement No. 609033. A.A.R. acknowledges financial support by the Spanish Ministry of Economy and Competitiveness through project AYA2014-60476-P and the Ramón y Cajal fellowships. J.C. thanks spanish MINECO for funding under grants AYA2012-32032, AYA2016-75066-C2-1-P, CSD2009-00038 (ASTROMOL) under the Consolider-Ingenio Program, and the European Research Council under the European Union’s Seventh Framework Programme (FP/2007-2013)/ERC-SyG-2013 Grant Agreement No. 610256 NANOCOSMOS. The support of the COST CMTS-Actions CM1405 (MOLIM: MOLecules In Motion) and CM1401 (Our Astro-Chemical History) is acknowledged.
Published: 2017
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24. The Genealogical Tree of Ethanol: Gas-phase Formation of Glycolaldehyde, Acetic Acid, and Formic Acid

Author: Fanny Vazart, Vincenzo Barone, Claudio Codella, Cecilia Ceccarelli, Nadia Balucani, Cristina Puzzarini, Bertrand Lefloch, Dimitrios Skouteris, Skouteris, Dimitrio, Balucani, Nadia, Ceccarelli, Cecilia, Vazart, Fanny, Puzzarini, Cristina, Barone, Vincenzo, Codella, Claudio, and Lefloch, Bertrand
Subjects: Physics, Astrochimica, Glycolaldehyde, Ethanol, 010304 chemical physics, Abundance (chemistry), Formic acid, Kinetics, FOS: Physical sciences, Astronomy and Astrophysics, 01 natural sciences, ISM: abundance, ISM: molecules, Interstellar medium, chemistry.chemical_compound, Acetic acid, chemistry, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Computational chemistry, 0103 physical sciences, Ethanol fuel, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: Despite the harsh conditions of the interstellar medium, chemistry thrives in it, especially in star forming regions where several interstellar complex organic molecules (iCOMs) have been detected. Yet, how these species are synthesised is a mystery. The majority of current models claim that this happens on interstellar grain surfaces. Nevertheless, evidence is mounting that neutral gas-phase chemistry plays an important role. In this article, we propose a new scheme for the gas-phase synthesis of glycolaldehyde, a species with a prebiotic potential and for which no gas-phase formation route was previously known. In the proposed scheme, the ancestor is ethanol and the glycolaldehyde sister species are acetic acid (another iCOM with unknown gas-phase formation routes) and formic acid. For the reactions of the new scheme with no available data, we have performed electronic structure and kinetics calculations deriving rate coefficients and branching ratios. Furthermore, after a careful review of the chemistry literature, we revised the available chemical networks, adding and correcting several reactions related to glycolaldehyde, acetic acid and formic acid. The new chemical network has been used in an astrochemical model to predict the abundance of glycolaldehyde, acetic acid and formic acid. The predicted abundance of glycolaldehyde depends on the ethanol abundance in the gas phase and is in excellent agreement with the measured one in hot corinos and shock sites. Our new model overpredicts the abundance of acetic acid and formic acid by about a factor of ten, which might imply a yet incomplete reaction network.
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24 results on '"Codella, Claudio"'

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24. The Genealogical Tree of Ethanol: Gas-phase Formation of Glycolaldehyde, Acetic Acid, and Formic Acid

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