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1. Linking the dust and chemical evolution: Taurus and Perseus: New collisional rates for HCN, HNC, and their C, N, and H isotopologues

Author

Navarro-Almaida, D., Bop, Cheikh T, Lique, François, Esplugues, G., Rodríguez-Baras, M., Kramer, Carsten, Romero, Charles, Fuente, A., Caselli, P., Rivière-Marichalar, P., Kirk, J., Chacón-Tanarro, A., Roueff, E., Mroczkowski, Tony, Bhandarkar, Tanay, Devlin, Mark, Dicker, Simon, Lowe, Ian, Mason, Brian, Sarazin, Craig, Sievers, Jonathan, Observatorio Astronomico Nacional, Madrid, Instituto Geografico Nacional (IGN), Institut de Physique de Rennes (IPR), Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS), Institut de RadioAstronomie Millimétrique (IRAM), Centre National de la Recherche Scientifique (CNRS), École Nationale des Travaux Publics de l'État (ENTPE), Max-Planck-Institut für Extraterrestrische Physik (MPE), School of Physics and Astronomy [Cardiff], Cardiff University, LERMA Cergy (LERMA), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), European Southern Observatory (ESO), University of Pennsylvania, University of Virginia, and McGill University = Université McGill [Montréal, Canada]

Subjects
[PHYS]Physics [physics], stars: formation, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], ISM: kinematic and dynamics, Molecular physics, ISM: abundances, ISM: molecules
Abstract

International audience; Context. HCN, HNC, and their isotopologues are ubiquitous molecules that can serve as chemical thermometers and evolutionary tracers to characterize star-forming regions. Despite their importance in carrying information that is vital to studies of the chemistry and evolution of star-forming regions, the collision rates of some of these molecules have not been available for rigorous studies in the past.Aims. Our goal is to perform an up-to-date gas and dust chemical characterization of two different star-forming regions, TMC 1-C and NGC 1333-C7, using new collisional rates of HCN, HNC, and their isotopologues. We investigated the possible effects of the environment and stellar feedback in their chemistry and their evolution. Methods. We used updated collisional rates of HCN, HNC, and their isotopologues in our analysis of the chemistry of TMC 1-C (Taurus) and NGC 1333-C7 (Perseus). With millimeter observations, we derived their column densities, the C and N isotopic fractions, the isomeric ratios, and the deuterium fractionation. The continuum data at 3 mm and 850 µm allowed us to compute the emissivity spectral index and look for grain growth as an evolutionary tracer.Results. The H 13 CN/HN 13 C ratio is anticorrelated with the deuterium fraction of HCN, thus it can readily serve as a proxy for the temperature. The spectral index ( β ~ 1.34–2.09) shows a tentative anticorrelation with the H 13 CN/HN 13 C ratio, suggesting grain growth in the evolved, hotter, and less deuterated sources. Unlike TMC 1-C, the south-to-north gradient in dust temperature and spectral index observed in NGC 1333-C7 suggests feedback from the main NGC 1333 cloud.Conclusions. With this up-to-date characterization of two star-forming regions, we found that the chemistry and the physical properties are tightly related. The dust temperature, deuterium fraction, and the spectral index are complementary evolutionary tracers. The large-scale environmental factors may dominate the chemistry and evolution in clustered star-forming regions.

Published
2023
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2. Discovery of CH3CHCO in TMC-1 with the QUIJOTE line survey

Author

R. Fuentetaja, C. Bermúdez, C. Cabezas, M. Agúndez, B. Tercero, N. Marcelino, J. R. Pardo, L. Margulès, R. A. Motiyenko, J.-C. Guillemin, P. de Vicente, J. Cernicharo, Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Universidad de Valladolid [Valladolid] (UVa), Instituto Geografico Nacional (IGN), Laboratoire de Physique des Lasers, Atomes et Molécules - UMR 8523 (PhLAM), Université de Lille-Centre National de la Recherche Scientifique (CNRS), Institut des Sciences Chimiques de Rennes (ISCR), Université de Rennes (UR)-Institut National des Sciences Appliquées - Rennes (INSA Rennes), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Ecole Nationale Supérieure de Chimie de Rennes (ENSCR)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Ministerio de Ciencia e Innovacion of Spain (MICIU) [PID2019-106110GB-I00, ERC-2013-Syg-610256-NANOCOSMOS], ERC [CONVREC-2021-317], Ministerio de Universidades [PID2019-107115GB-C21], and [PID2019-106235GB-I00]

Subjects
individual objects, molecular data, astrochemistry, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, TMC-1, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), identification, [CHIM]Chemical Sciences, line, molecules, ISM
Abstract

We report the detection of methyl ketene towards TMC-1 with the QUIJOTE line survey. Nineteen rotational transitions with rotational quantum numbers ranging from J = 3 up to J = 5 and Ka ≤ 2 were identified in the frequency range 32.0–50.4 GHz, 11 of which arise above the 3σ level. We derived a column density for CH3CHCO of N = 1.5 × 1011 cm−2 and a rotational temperature of 9 K. Hence, the abundance ratio between ketene and methyl ketene, CH2CO/CH3CHCO, is 93. This species is the second C3H4O isomer detected. The other, trans-propenal (CH2CHCHO), corresponds to the most stable isomer and has a column density of N = (2.2 ± 0.3)×1011 cm−2, which results in an abundance ratio CH2CHCHO/CH3CHCO of 1.5. The next non-detected isomer with the lowest energy is cis-propenal, which is therefore a good candidate for future discovery. We have carried out an in-depth study of the possible gas-phase chemical reactions involving methyl ketene to explain the abundance detected, achieving good agreement between chemical models and observations.

Published
2023
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3. Towards the new Thematic Core Service Tsunami within the EPOS Research Infrastructure

Author

Andrey Babeyko, Stefano Lorito, Francisco Hernandez, Jörn Lauterjung, Finn Løvholt, Alexander Rudloff, Mathilde Sørensen, Alexey Androsov, Inigo Aniel-Quiroga, Alberto Armigliato, Maria Ana Baptista, Enrico Baglione, Roberto Basili, Jörn Behrens, Beatriz Brizuela, Sergio Bruni, Didem Cambaz, Juan Cantavella Nadal, Fernando Carillho, Ian Chandler, Denis Chang-Seng, Marinos Charalampakis, Lorenzo Cugliari, Clea Denamiel, Gözde Güney Doğan, Gaetano Festa, David Fuhrman, Alice-Agnes Gabriel, Pauline Galea, Steven Gibbons, Mauricio González, Laura Graziani, Marc-André Gutscher, Sven Harig, Helene Hebert, Constantin Ionescu, Fatemeh Jalayer, Nikos Kalligeris, Utku Kânoğlu, Piero Lanucara, Jorge Macias Sánchez, Shane Murphy, Öcal Necmioğlu, Rachid Omira, Gerassimos Papadopoulos, Raphaël Paris, Fabrizio Romano, Tiziana Rossetto, Jacopo Selva, Antonio Scala, Roberto Tonini, Konstantinos Trevlopoulos, Ioanna Triantafyllou, Roger Urgeles, Roberto Vallone, Ivica Vilibić, Manuela Volpe, Ahmet Yalciner, Agencia Estatal de Investigación (España), Andrey Babeyko, Stefano Lorito, Francisco Hernandez, Jörn Lauterjung, Finn Løvholt, Alexander Rudloff, Mathilde Sørensen, Alexey Androsov, Inigo Aniel-Quiroga, Alberto Armigliato, Maria Ana Baptista, Enrico Baglione, Roberto Basili, Jörn Behrens, Beatriz Brizuela, Sergio Bruni, M. Didem Cambaz, Juan Cantavella-Nadal, Fernando Carrilho, Ian Chandler, Denis Chang-Seng, Marinos Charalampakis, Lorenzo Cugliari, Clea Denamiel, Gözde Güney Dogan, Gaetano Festa, David Fuhrman, Alice-Agnes Gabriel, Pauline Galea, Steven J. Gibbons, Mauricio Gonzalez, Laura Graziani, Marc-André Gutscher, Sven Harig, Helen Hebert, Constantin Ionescu, Fatemeh Jalayer, Nikos Kalligeris, Utku Kânoğlu, Piero Lanucara, Jorge Macías Sánchez, Shane Murphy, Öcal Necmioğlu, Rachid Omira, Gerassimos A. Papadopoulos, Raphaël Paris, Fabrizio Romano, Tiziana Rossetto, Jacopo Selva, Antonio Scala, Roberto Tonini, Konstantinos Trevlopoulos, Ioanna Triantafyllou, Roger Urgeles, Roberto Vallone, Ivica Vilibić, Manuela Volpe, Ahmet C. Yalciner, GeoForschungsZentrum - Helmholtz-Zentrum Potsdam (GFZ), Istituto Nazionale di Geofisica e Vulcanologia, Flanders Marine Institute (VLIZ), Norwegian Geotechnical Institute (NGI), University of Bergen (UiB), Alfred Wegener Institute [Potsdam], Alfred-Wegener-Institut, Helmholtz-Zentrum für Polar- und Meeresforschung (AWI), IHCantabria - Instituto de Hidráulica Ambiental de La Universidad de Cantabria, Santander, Alma Mater Studiorum University of Bologna (UNIBO), Instituto Superior de Engenharia de Lisboa (ISEL), Universität Hamburg (UHH), Kandilli Observatory and Earthquake Research Institute (KOERI), Boǧaziçi üniversitesi = Boğaziçi University [Istanbul], Instituto Geografico Nacional (IGN), Instituto Português de Investigação do Mar e da Atmosfera (IPMA), HR Wallingford Limited, Intergovernmental Oceanographic Commission of UNESCO, Institute of Geodynamics [Athens], National Observatory of Athens (NOA), Institut Ruđer Bošković (IRB), Middle East Technical University [Ankara] (METU), University of Naples Federico II = Università degli studi di Napoli Federico II, Danmarks Tekniske Universitet = Technical University of Denmark (DTU), Ludwig-Maximilians-Universität München (LMU), University of Malta [Malta], Geo-Ocean (GEO-OCEAN), Université de Bretagne Sud (UBS)-Institut Français de Recherche pour l'Exploitation de la Mer (IFREMER)-Université de Brest (UBO)-Centre National de la Recherche Scientifique (CNRS), DAM Île-de-France (DAM/DIF), Direction des Applications Militaires (DAM), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), National Institute for Earth Physics [Romania] - Institutul Național pentru Fizica Pământului (NIEP), CINECA Consorzio Interuniversitario [Rome, Italy], Universidad de Málaga [Málaga] = University of Málaga [Málaga], International Society for the Prevention and Mitigation of Natural Hazards, Athens, Observatoire de Physique du Globe de Clermont-Ferrand (OPGC), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Clermont Auvergne (UCA), University College of London [London] (UCL), Department of Geology and Geoenvironment, National and Kapodistrian University of Athens (NKUA), Centre d'Investigació i Desenvolupament [Barcelona] (CID-CSIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), European Project: 262229,EC:FP7:INFRA,FP7-INFRASTRUCTURES-2010-1,EPOS(2010), and Universidad de Cantabria

Subjects
[SDU.OCEAN]Sciences of the Universe [physics]/Ocean, Atmosphere, Geophysics, Tsunami, Natural hazards, Community building, EPOS, Research infrastructure, Tsunami Natural hazards Community building EPOS Research infrastructure
Abstract

Special issue EPOS a Research Infrastructure in solid Earth: open science and innovation .-- 21 pages, 8 figures, Tsunamis constitute a significant hazard for European coastal populations, and the impact of tsunami events worldwide can extend well beyond the coastal regions directly affected. Understanding the complex mechanisms of tsunami generation, propagation, and inundation, as well as managing the tsunami risk, requires multidisciplinary research and infrastructures that cross national boundaries. Recent decades have seen both great advances in tsunami science and consolidation of the European tsunami research community. A recurring theme has been the need for a sustainable platform for coordinated tsunami community activities and a hub for tsunami services. Following about three years of preparation, in July 2021, the European tsunami community attained the status of Candidate Thematic Core Service (cTCS) within the European Plate Observing System (EPOS) Research Infrastructure. Within a transition period of three years, the Tsunami candidate TCS is anticipated to develop into a fully operational EPOS TCS. We here outline the path taken to reach this point, and the envisaged form of the future EPOS TCS Tsunami. Our cTCS is planned to be organised within four thematic pillars: (1) Support to Tsunami Service Providers, (2) Tsunami Data, (3) Numerical Models, and (4) Hazard and Risk Products. We outline how identified needs in tsunami science and tsunami risk mitigation will be addressed within this structure and how participation within EPOS will become an integration point for community development, With the institutional support of the ‘Severo Ochoa Centre of Excellence’ accreditation (CEX2019-000928-S)

Published
2022
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4. SOLIS XVI. Mass ejection and time variability in protostellar outflows: Cep E

Author

A. de A. Schutzer, P. R. Rivera-Ortiz, B. Lefloch, A. Gusdorf, C. Favre, D. Segura-Cox, A. López-Sepulcre, R. Neri, J. Ospina-Zamudio, M. De Simone, C. Codella, S. Viti, L. Podio, J. Pineda, R. O’Donoghue, C. Ceccarelli, P. Caselli, F. Alves, R. Bachiller, N. Balucani, E. Bianchi, L. Bizzocchi, S. Bottinelli, E. Caux, A. Chacón-Tanarro, F. Dulieu, J. Enrique-Romero, F. Fontani, S. Feng, J. Holdship, I. Jiménez-Serra, A. Jaber Al-Edhari, C. Kahane, V. Lattanzi, Y. Oya, A. Punanova, A. Rimola, N. Sakai, S. Spezzano, I. R. Sims, V. Taquet, L. Testi, P. Theulé, P. Ugliengo, C. Vastel, A. I. Vasyunin, F. Vazart, S. Yamamoto, A. Witzel, A. de A. Schutzer, P. R. Rivera-Ortiz, B. Lefloch, A. Gusdorf, C. Favre, D. Segura-Cox, A. L??pez-Sepulcre, R. Neri, J. Ospina-Zamudio, M. De Simone, C. Codella, S. Viti, L. Podio, J. Pineda, R. O'Donoghue, C. Ceccarelli, P. Caselli, F. Alve, R. Bachiller, N. Balucani, E. Bianchi, L. Bizzocchi, S. Bottinelli, E. Caux, A. Chacón-Tanarro, F. Dulieu, J. Enrique-Romero, F. Fontani, S. Feng, J. Holdship, I. Jiménez-Serra, A. Jaber Al-Edhari, C. Kahane, V. Lattanzi, Y. Oya, A. Punanova, A. Rimola, N. Sakai, S. Spezzano, I. R. Sim, V. Taquet, L. Testi, P. Theulé, P. Ugliengo, C. Vastel, A. I. Vasyunin, F. Vazart, S. Yamamoto, A. Witzel, 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, Observatoire de Paris, Université Paris sciences et lettres (PSL), Astrophysique, Laboratoire de physique de l'ENS - ENS Paris (LPENS), Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), 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)-Département de Physique de l'ENS-PSL, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Centre de Mathématiques Laurent Schwartz (CMLS), École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Extraterrestrische Physik (MPE), University of Texas at Austin [Austin], Institut de RadioAstronomie Millimétrique (IRAM), Centre National de la Recherche Scientifique (CNRS), University College of London [London] (UCL), INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), Laboratoire de Radiopathologie (LRP), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de la Santé et de la Recherche Médicale (INSERM), Observatorio Astronomico Nacional, Madrid, Dip. Chimica 'G. Ciamician', Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), 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), Instituto Geografico Nacional (IGN), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), The University of Tokyo (UTokyo), Ural Federal University [Ekaterinburg] (UrFU), Universitat Autònoma de Barcelona (UAB), RIKEN - Institute of Physical and Chemical Research [Japon] (RIKEN), Institut de Physique de Rennes (IPR), Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS), Physique des interactions ioniques et moléculaires (PIIM), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS), Università degli studi di Torino = University of Turin (UNITO), Based on observations carried out with the IRAM NOEMA interferometer. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain). AS, BL, PR-RO, acknowledge support from the European Union’s Horizon 2020 research and innovation program under the Marie Skłodowska-Curie grant agreement No 811312 for the project 'Astro-Chemical Origins' (ACO) and the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program for the Project 'The Dawn of Organic Chemistry' (DOC) grant agreement No 741002. DSC is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-2102405. A.V. and A.P. are the members of the Max Planck Partner Group at the Ural Federal University. A.P. and A.V. acknowledge the support of the Russian Ministry of Science and Education via the State Assignment Contract no. FEUZ-2020-0038., European Project: 811312, LERMA Cergy (LERMA), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères (LERMA (UMR_8112)), 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)-CY Cergy Paris Université (CY)-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)-CY Cergy Paris Université (CY), INSU/CNRS (France), MPG (Germany), IGN (Spain), European Union [811312], European Research Council (ERC) under the European Union [741002], NSF Astronomy and Astrophysics Postdoctoral Fellowship [AST-2102405], and Russian Ministry of Science and Education [FEUZ-2020-0038]

Subjects
DYNAMICS, MASS EJECTION, JETS AND OUTFLOWS [ISM], KINEMATICS AND DYNAMICS [ISM], ISM JETS AND OUTFLOWS, TIME VARIABILITY, JET FORMATION, HIGH VELOCITY, FORMATION [STARS], ISM: kinematics and dynamic, KINEMATICS, ISM: jets and outflow, ISM: kinematics and dynamics, stars: formation, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], astrochemistry, STARS FORMATION, ACCRETION PROCESS, PROTOSTARS, Astronomy and Astrophysics, VELOCITY, MASS LOSS RATE, Astrophysics - Astrophysics of Galaxies, ISM: jets and outflows, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], STARS
Abstract

Context. Protostellar jets are an important agent of star formation feedback, tightly connected with the mass-accretion process. The history of jet formation and mass ejection provides constraints on the mass accretion history and on the nature of the driving source. Aims. We characterize the time-variability of the mass-ejection phenomena at work in the class 0 protostellar phase in order to better understand the dynamics of the outflowing gas and bring more constraints on the origin of the jet chemical composition and the mass accretion history. Methods. Using the NOrthern Extended Millimeter Array (NOEMA) interferometer, we have observed the emission of the CO 2–1 and SO NJ = 54–43 rotational transitions at an angular resolution of 1.0 00 (820 au) and 0.400 (330 au), respectively, toward the intermediate mass class 0 protostellar system Cep E. Results. The CO high-velocity jet emission reveals a central component of ≤400 au diameter associated with high-velocity molecular knots that is also detected in SO, surrounded by a collimated layer of entrained gas. The gas layer appears to be accelerated along the main axis over a length scale δ0 ∼ 700 au, while its diameter gradually increases up to several 1000 au at 2000 au from the protostar. The jet is fragmented into 18 knots of mass ∼10−3 M, unevenly distributed between the northern and southern lobes, with velocity variations up to 15 km s−1 close to the protostar. This is well below the jet terminal velocities in the northern (+65 km s−1) and southern (-125 km s-1)lobes. The knot interval distribution is approximately bimodal on a timescale of ∼50–80 yr, which is close to the jet driving protostar Cep E-A and ∼150−20 yr at larger distances >1200. The mass-loss rates derived from knot masses are steady overall, with values of 2.7 x 10−5 M yr−1 and 8.9 x 10−6 M yr−1 in the northern and southern lobe, respectively. Conclusions. The interaction of the ambient protostellar material with high-velocity knots drives the formation of a molecular layer around the jet. This accounts for the higher mass-loss rate in the northern lobe. The jet dynamics are well accounted for by a simple precession model with a period of 2000 yr and a mass-ejection period of 55 yr. © Authors 2022 741002; National Science Foundation, NSF: AST-2102405; Horizon 2020 Framework Programme, H2020; H2020 Marie Skłodowska-Curie Actions, MSCA: 811312; European Research Council, ERC; Ministry of Education and Science of the Russian Federation, Minobrnauka: FEUZ-2020-0038; Centre National de la Recherche Scientifique, CNRS; Ural Federal University, UrFU interferometer. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain). AS, BL, PR-RO, acknowledge support from the European Union’s Horizon 2020 research and innovation program under the Marie Skłodowska-Curie grant agreement No 811312 for the project “Astro-Chemical Origins” (ACO) and the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program for the Project “The Dawn of Organic Chemistry” (DOC) grant agreement No 741002. DSC is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-2102405. A.V. and A.P. are the members of the Max Planck Partner Group at the Ural Federal University. A.P. and A.V. acknowledge the support of the Russian Ministry of Science and Education via the State Assignment Contract no. FEUZ-2020-0038. Based on observations carried out with the IRAM NOEMA interferometer. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain). AS, BL, PR-RO, acknowledge support from the European Union’s Horizon 2020 research and innovation program under the Marie Skłodowska-Curie grant agreement No 811312 for the project "Astro-Chemical Origins" (ACO) and the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program for the Project "The Dawn of Organic Chemistry" (DOC) grant agreement No 741002. DSC is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-2102405. A.V. and A.P. are the members of the Max Planck Partner Group at the Ural Federal University. A.P. and A.V. acknowledge the support of the Russian Ministry of Science and Education via the State Assignment Contract no. FEUZ-2020-0038.

Published
2022
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